FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Gioia, J Yerrapragada, S Qin, X Jiang, HY Igboeli, OC Muzny, D Dugan-Rocha, S Ding, Y Hawes, A Liu, W Perez, L Kovar, C Dinh, H Lee, S Nazareth, L Blyth, P Holder, M Buhay, C Tirumalai, MR Liu, YM Dasgupta, I Bokhetache, L Fujita, M Karouia, F Moorthy, PE Siefert, J Uzman, A Buzumbo, P Verma, A Zwiya, H McWilliams, BD Olowu, A Clinkenbeard, KD Newcombe, D Golebiewski, L Petrosino, JF Nicholson, WL Fox, GE Venkateswaran, K Highlander, SK Weinstock, GM AF Gioia, Jason Yerrapragada, Shailaja Qin, Xiang Jiang, Huaiyang Igboeli, Okezie C. Muzny, Donna Dugan-Rocha, Shannon Ding, Yan Hawes, Alicia Liu, Wen Perez, Lesette Kovar, Christie Dinh, Huyen Lee, Sandra Nazareth, Lynne Blyth, Peter Holder, Michael Buhay, Christian Tirumalai, Madhan R. Liu, Yamei Dasgupta, Indrani Bokhetache, Lina Fujita, Masaya Karouia, Fathi Moorthy, Prahathees Eswara Siefert, Johnathan Uzman, Akif Buzumbo, Prince Verma, Avani Zwiya, Hiba McWilliams, Brian D. Olowu, Adeola Clinkenbeard, Kenneth D. Newcombe, David Golebiewski, Lisa Petrosino, Joseph F. Nicholson, Wayne L. Fox, George E. Venkateswaran, Kasthuri Highlander, Sarah K. Weinstock, George M. TI Paradoxical DNA Repair and Peroxide Resistance Gene Conservation in Bacillus pumilus SAFR-032 SO PLOS ONE LA English DT Article AB Background. Bacillus spores are notoriously resistant to unfavorable conditions such as UV radiation, gamma-radiation, H(2)O(2), desiccation, chemical disinfection, or starvation. Bacillus pumilus SAFR-032 survives standard decontamination procedures of the Jet Propulsion Lab spacecraft assembly facility, and both spores and vegetative cells of this strain exhibit elevated resistance to UV radiation and H(2)O(2) compared to other Bacillus species. Principal Findings. The genome of B. pumilus SAFR-032 was sequenced and annotated. Lists of genes relevant to DNA repair and the oxidative stress response were generated and compared to B. subtilis and B. licheniformis. Differences in conservation of genes, gene order, and protein sequences are highlighted because they potentially explain the extreme resistance phenotype of B. pumilus. The B. pumilus genome includes genes not found in B. subtilis or B. licheniformis and conserved genes with sequence divergence, but paradoxically lacks several genes that function in UV or H(2)O(2) resistance in other Bacillus species. Significance. This study identifies several candidate genes for further research into UV and H(2)O(2) resistance. These findings will help explain the resistance of B. pumilus and are applicable to understanding sterilization survival strategies of microbes. C1 [Gioia, Jason; Yerrapragada, Shailaja; Qin, Xiang; Jiang, Huaiyang; Igboeli, Okezie C.; Muzny, Donna; Dugan-Rocha, Shannon; Ding, Yan; Hawes, Alicia; Liu, Wen; Perez, Lesette; Kovar, Christie; Dinh, Huyen; Lee, Sandra; Nazareth, Lynne; Blyth, Peter; Holder, Michael; Buhay, Christian; Highlander, Sarah K.; Weinstock, George M.] Baylor Coll Med, Human Genome Sequencing Ctr, Houston, TX 77030 USA. [Weinstock, George M.] Baylor Coll Med, Dept Mol & Human Genet, Houston, TX 77030 USA. [McWilliams, Brian D.; Golebiewski, Lisa; Petrosino, Joseph F.; Highlander, Sarah K.; Weinstock, George M.] Baylor Coll Med, Dept Mol Virol & Microbiol, Houston, TX 77030 USA. [Tirumalai, Madhan R.; Liu, Yamei; Dasgupta, Indrani; Bokhetache, Lina; Fujita, Masaya; Karouia, Fathi; Moorthy, Prahathees Eswara; Siefert, Johnathan; Fox, George E.] Univ Houston, Dept Biol & Biochem, Houston, TX USA. [Uzman, Akif; Buzumbo, Prince; Verma, Avani; Zwiya, Hiba] Univ Houston Downtown, Dept Nat Sci, Houston, TX USA. [Olowu, Adeola] St Thomas Univ, Houston, TX USA. [Clinkenbeard, Kenneth D.] Oklahoma State Univ, Dept Vet Pathobiol, Ctr Vet Hlth Sci, Stillwater, OK 74078 USA. [Newcombe, David] Univ Idaho Coeur dAlene, Coeur Dalene, ID USA. [Newcombe, David; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Nicholson, Wayne L.] Univ Florida, Space Life Sci Lab, Dept Microbiol & Cell Sci, Kennedy Space Ctr, FL USA. RP Weinstock, GM (reprint author), Baylor Coll Med, Human Genome Sequencing Ctr, Houston, TX 77030 USA. EM gwstock@bcm.tmc.edu OI R Tirumalai, Madhan/0000-0002-5999-333X FU NSF [414410]; NASA [NNG05GN75G]; NRA ROSS FX This research was supported in part by grants to GMW (NSF-414410), GEF (NASA-Exobiology #NNG05GN75G) and KV (contract to JPL/Caltech from NASA and funded by NRA ROSS 2005). The sponsors had no role in the conduct of this study. NR 70 TC 69 Z9 496 U1 0 U2 21 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 26 PY 2007 VL 2 IS 9 AR e928 DI 10.1371/journal.pone.0000928 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA V10HT UT WOS:000207455800007 PM 17895969 ER PT J AU Schull, MA Ganguly, S Samanta, A Huang, D Shabanov, NV Jenkins, JP Chiu, JC Marshak, A Blair, JB Myneni, RB Knyazikhin, Y AF Schull, M. A. Ganguly, S. Samanta, A. Huang, D. Shabanov, N. V. Jenkins, J. P. Chiu, J. C. Marshak, A. Blair, J. B. Myneni, R. B. Knyazikhin, Y. TI Physical interpretation of the correlation between multi-angle spectral data and canopy height SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RADIATION; COVER; MODIS; MISR; INVARIANTS; SCALES; MODEL; LIDAR; LEAF AB Recent empirical studies have shown that multi-angle spectral data can be useful for predicting canopy height, but the physical reason for this correlation was not understood. We follow the concept of canopy spectral invariants, specifically escape probability, to gain insight into the observed correlation. Airborne Multi-Angle Imaging Spectrometer (AirMISR) and airborne Laser Vegetation Imaging Sensor (LVIS) data acquired during a NASA Terrestrial Ecology Program aircraft campaign underlie our analysis. Two multivariate linear regression models were developed to estimate LVIS height measures from 28 AirMISR multi-angle spectral reflectances and from the spectrally invariant escape probability at 7 AirMISR view angles. Both models achieved nearly the same accuracy, suggesting that canopy spectral invariant theory can explain the observed correlation. We hypothesize that the escape probability is sensitive to the aspect ratio (crown diameter to crown height). The multi-angle spectral data alone therefore may not provide enough information to retrieve canopy height globally. C1 Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA. Brookhaven Natl Lab, Div Atmospher Sci, Upton, NY 11973 USA. Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03824 USA. NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. RP Schull, MA (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA. EM schull@bu.edu; sganguly@bu.edu; arindam@bu.edu; dhuang@bnl.gov; shabanov@bu.edu; julian.jenkins@unh.edu; cchiu@climate.gsfc.nasa.gov; alexander.marshak@nasa.gov; james.b.blair@nasa.gov; rmyneni@bu.edu; jknjazi@bu.edu RI Schull, Mitch/D-1663-2010; Samanta, Arindam/B-9550-2009; Myneni, Ranga/F-5129-2012; Khachadourian, Diana/C-8513-2012; Marshak, Alexander/D-5671-2012; Blair, James/D-3881-2013; Chiu, Christine/E-5649-2013; Huang, Dong/H-7318-2014; ganguly, sangram/B-5108-2010 OI Chiu, Christine/0000-0002-8951-6913; Huang, Dong/0000-0001-9715-6922; NR 28 TC 23 Z9 24 U1 3 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 25 PY 2007 VL 34 IS 18 AR L18405 DI 10.1029/2007GL031143 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 216AS UT WOS:000249850700004 ER PT J AU Warren-Rhodes, K Weinstein, S Piatek, JL Dohm, J Hock, A Minkley, E Pane, D Ernst, LA Fisher, G Emani, S Waggoner, AS Cabrol, NA Wettergreen, DS Grin, E Coppin, P Diaz, C Moersch, J Oril, GG Smith, T Stubbs, K Thomas, G Wagner, M Wyatt, M Boyle, LN AF Warren-Rhodes, K. Weinstein, S. Piatek, J. L. Dohm, J. Hock, A. Minkley, E. Pane, D. Ernst, L. A. Fisher, G. Emani, S. Waggoner, A. S. Cabrol, N. A. Wettergreen, D. S. Grin, E. Coppin, P. Diaz, Chong Moersch, J. Oril, G. G. Smith, T. Stubbs, K. Thomas, G. Wagner, M. Wyatt, M. Boyle, L. Ng TI Robotic ecological mapping: Habitats and the search for life in the Atacama Desert SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID SOIL-MOISTURE; VEGETATION; CHILE; ECOHYDROLOGY; DYNAMICS; CLIMATE; SCALES AB [ 1] As part of the three-year 'Life in the Atacama' ( LITA) project, plant and microbial abundance were mapped within three sites in the Atacama Desert, Chile, using an automated robotic rover. On-board fluorescence imaging of six biological signatures ( e. g., chlorophyll, DNA, proteins) was used to assess abundance, based on a percent positive sample rating system and standardized robotic ecological transects. The percent positive rating system scored each sample based on the measured signal strength ( 0 for no signal to 2 for strong signal) for each biological signature relative to the total rating possible. The 2005 field experiment results show that percent positive ratings varied significantly across Site D ( coastal site with fog), with patchy zones of high abundance correlated with orbital and microscale habitat types ( heaved surface crust and gravel bars); alluvial fan habitats generally had lower abundance. Non-random multi-scale biological patchiness also characterized interior desert Sites E and F, with relatively high abundance associated with (paleo) aqueous habitats such as playas. Localized variables, including topography, played an important, albeit complex, role in microbial spatial distribution. Site D biosignature trends correlated with culturable soil bacteria, with MPN ranging from 10-1000 CFU/ g-soil, and chlorophyll ratings accurately mapped lichen/moss abundance ( Site D) and higher plant ( Site F) distributions. Climate also affected biological patchiness, with significant correlation shown between abundance and ( rover) air relative humidity, while lichen patterns were linked to the presence of fog. Rover biological mapping results across sites parallel longitudinal W-E wet/dry/wet Atacama climate trends. Overall, the study highlights the success of targeting of aqueous-associated habitats identifiable from orbital geology and mineralogy. The LITA experience also suggests the terrestrial study of life and its distribution, particularly the fields of landscape ecology and ecohydrology, hold critical lessons for the search for life on other planets. Their applications to robotic sampling strategies on Mars should be further exploited. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. Univ Iowa, Dept Mech & Ind Engn, Iowa City, IA 52242 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. SETI Inst, Mountain View, CA 94043 USA. Carnegie Mellon Univ, Mol Biosensor & Imaging Ctr, Pittsburgh, PA 15213 USA. Univ Catolica Norte, Antofagasta, Chile. RP Warren-Rhodes, K (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM kwarren-rhodes@mail.arc.nasa.gov RI Moersch, Jeffrey/F-7189-2010; Dohm, James/A-3831-2014 NR 37 TC 8 Z9 8 U1 1 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD SEP 25 PY 2007 VL 112 IS G4 AR G04S06 DI 10.1029/2006JG000301 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 216BL UT WOS:000249852700001 ER PT J AU Klemann, V Ivins, ER Martinec, Z Wolf, D AF Klemann, Volker Ivins, Erik R. Martinec, Zdenek Wolf, Detlef TI Models of active glacial isostasy roofing warm subduction: Case of the South Patagonian Ice Field SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID MANTLE; AMERICA; HOLOCENE; FLUCTUATIONS; CRUSTAL AB Modern geodetic techniques such as precise Global Positioning System ( GPS) and high-resolution space gravity mapping ( Gravity Recovery and Climate Experiment, GRACE) make it possible to measure the present-day rate of viscoelastic gravitational Earth response to present and past glacier mass changes. The Andes of Patagonia contain glacial environments of dramatic mass change. These mass load changes occur near a tectonically active boundary between the Antarctic and South American plates. The mechanical strength of the continental side of this boundary is influenced by Neogene ridge subduction and by the subduction of a youthful oceanic slab. A ridge of young volcanos parallels the Pacific coastline. Release of volatiles ( such as water) at depth along this ridge creates a unique rheological environment. To assess the influence of this rheological ridge structure on the observational land uplift rate, we apply a two-dimensional viscoelastic Earth model. A numerical study is presented which examines the sensitivity of the glacial loading-unloading response to the complex structure at depth related to the subducting slab, the viscous wedge between slab and continental lithosphere, and the increase of elastic thickness from oceanic to continental lithosphere. A key feature revealed by our numerical experiments is a continuum flow wherein the slab subdues the material transport toward oceanic mantle and crust. The restricted flow is sensitive to the details of slab mechanical strength and penetration into the upper mantle. The reduced viscosity within the mantle wedge, however, enhances the load-induced material transport everywhere within the asthenosphere. C1 Geoforschungszentrum Potsdam, Geodesy & Remote Sensing, Potsdam, Germany. CALTECH, Jet Prop Lab, Pasadena, CA USA. Charles Univ Prague, Dept Geophys, Prague, Czech Republic. Univ Stuttgart, Geo Inst, Stuttgart, Germany. RP Klemann, V (reprint author), Geoforschungszentrum Potsdam, Geodesy & Remote Sensing, Potsdam, Germany. EM volkerk@gfz-potsdam.de; erik.r.ivins@jpl.nasa.gov; zdenek@gfz-potsdam.de; dasca@gfz-potsdam.de RI Klemann, Volker/H-3660-2013 OI Klemann, Volker/0000-0002-8342-8947 NR 25 TC 20 Z9 20 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD SEP 25 PY 2007 VL 112 IS B9 AR B09405 DI 10.1029/2006JB004818 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 216BY UT WOS:000249854000001 ER PT J AU Yu, B Ju, SY Sun, XH Ng, G Nguyen, TD Meyyappan, M Janes, DB AF Yu, Bin Ju, Sanghyun Sun, Xuhui Ng, Garrick Nguyen, Thuc Dinh Meyyappan, M. Janes, David B. TI Indium selenide nanowire phase-change memory SO APPLIED PHYSICS LETTERS LA English DT Article AB Nonvolatile memory device using indium selenide nanowire as programmable resistive element was fabricated and its resistive switching property was studied as functions of electrical pulse width and voltage magnitude. The nanowire memory can be repeatedly switched between high-resistance (similar to 10(11) Omega) and low-resistance (similar to 6x10(5) Omega) states which are attributed to amorphous and crystalline states, respectively. Once set to a specific state, the nanowire resistance is stable as measured at voltages up to 2 V. This observation suggests that the nanowire can be programed into two distinct states with a large on-off resistance ratio of similar to 10(5) with significant potential for nonvolatile information storage. (C) 2007 American Institute of Physics. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Purdue Univ, Sch Elect & Comp Engn, Birck Nanotechnol Ctr, W Lafayette, IN 47907 USA. RP Yu, B (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM byu@arc.nasa.gov; xsun@arc.nasa.gov RI Sun, Xuhui /K-5689-2012 NR 10 TC 57 Z9 59 U1 4 U2 24 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 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD SEP 24 PY 2007 VL 91 IS 13 AR 133119 DI 10.1063/1.2793505 PG 3 WC Physics, Applied SC Physics GA 215CX UT WOS:000249787000097 ER PT J AU Tedesco, M Abdalati, W Zwally, HJ AF Tedesco, M. Abdalati, W. Zwally, H. J. TI Persistent surface snowmelt over Antarctica (1987-2006) from 19.35 GHz brightness temperatures SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VARIABILITY; TRENDS; MELT AB [1] Persistent melting ( e. g., continuing for more than three days or for one consecutive day and night) is mapped in Antarctica ( 1987-2006) using night- and day- time Special Sensor Microwave Imager brightness temperatures ( Tb) at 19.35 GHz, horizontal polarization. Snowmelt is indicated when Tb and relative daily difference exceed threshold values, respectively Tc and Delta T, computed for each pixel and year, or when both daytime and nighttime Tb exceed Tc. Results from an electromagnetic model suggest that the minimum detectable liquid water content ranges between 0.2 and 0.5%, in volume. We find that melting areas have been moving inland since 1987. A first-time extensive melting ( 1987-2006) is detected over the Transantarctic Mountains on January 2005, 875 Km inland and 2000 m above sea level. Melting extent and index have been decreasing over Antarctica, since 1987, although either positive and negative trends are observed from a subcontinental scale analysis. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. RP Tedesco, M (reprint author), NASA, Goddard Space Flight Ctr, Code 614-6, Greenbelt, MD 20771 USA. RI Tedesco, Marco/F-7986-2015 NR 13 TC 16 Z9 16 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 22 PY 2007 VL 34 IS 18 AR L18504 DI 10.1029/2007GL031199 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 213RG UT WOS:000249684200005 ER PT J AU Liu, HL Li, T She, CY Oberheide, J Wu, Q Hagan, ME Xu, J Roble, RG Mlynczak, MG Russell, JM AF Liu, H.-L. Li, T. She, C.-Y. Oberheide, J. Wu, Q. Hagan, M. E. Xu, J. Roble, R. G. Mlynczak, M. G. Russell, J. M., III TI Comparative study of short-term diurnal tidal variability SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; DOPPLER INTERFEROMETER TIDI; LATENT-HEAT RELEASE; PLANETARY-WAVES; NONMIGRATING TIDES; LOWER THERMOSPHERE; GRAVITY-WAVE; SEMIDIURNAL TIDES; MIDDLE ATMOSPHERE; MESOPAUSE REGION AB The wind and temperature measurements from an unusually long period operation of the sodium lidar at Colorado State University (41 degrees N, 105 degrees W) around September equinox 2003 showed significant short-term tidal variability. Coincident with the large tidal changes, a strong temperature inversion layer was also observed above 90 km. Examination of the simultaneous temperature measurement from the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument, on board the Thermosphere Ionosphere Mesosphere Energetics and Dynamics ( TIMED) satellite, not only confirms the existence of the inversion layer but also reveals the global nature of the inversion, suggesting the presence of a transient planetary wave in the mesosphere. The large tidal variability, therefore, is probably a consequence of the interaction between the transient planetary wave and tides. This possibility is investigated by using the NCAR thermosphere-ionosphere-mesosphere-electrodynamics general circulation model (TIME-GCM) and by comparing model results with the lidar, SABER, and TIMED Doppler Interferometer (TIDI) measurements. With a large transient planetary wave specified at the model lower boundary, the model is able to produce strong diurnal tidal variability comparable to that from the lidar observation, and the modeled temperature inversion is similar to that from the SABER measurement. The model results suggest that the planetary/tidal wave interaction excites nonmigrating tides and modulates the gravity modes and/or the rotational modes of the diurnal migrating tide. Among the nonmigrating tides, the diurnal zonally symmetric (S = 0) component is the strongest, and its interaction with the planetary wave leads to a strong diurnal eastward wave number 1 component. C1 Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Wuppertal Univ, Dept Phys, D-42119 Wuppertal, Germany. Hampton Univ, Dept Phys, Hampton, VA 23668 USA. Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA. Chinese Acad Sci, State Key Lab Space Weather, Beijing 100080, Peoples R China. RP Liu, HL (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA. EM liuh@ucar.edu RI Liu, Han-Li/A-9549-2008; Hagan, Maura/C-7200-2008; Oberheide, Jens/C-6156-2011; Mlynczak, Martin/K-3396-2012; Li, Tao/J-8950-2014 OI Liu, Han-Li/0000-0002-6370-0704; Hagan, Maura/0000-0002-8866-7429; Oberheide, Jens/0000-0001-6721-2540; Li, Tao/0000-0002-5100-4429 NR 60 TC 33 Z9 34 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 22 PY 2007 VL 112 IS D18 AR D18108 DI 10.1029/2007JD008542 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 213RW UT WOS:000249685800002 ER PT J AU Papa, F Prigent, C Rossow, WB AF Papa, F. Prigent, C. Rossow, W. B. TI Ob' River flood inundations from satellite observations: A relationship with winter snow parameters and river runoff SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INTERANNUAL VARIABILITY; WETLAND DYNAMICS; DISCHARGE; BASIN; ALGORITHM; PROJECT; MODEL; SSM/I; AREA AB Using a multisatellite method, including passive microwave land surface emissivities, along with active microwave, visible and near infrared observations developed to estimate global inundated area, we examine the spatial and temporal variations of the 1993 2000 monthly inundation extents over a Boreal environment, the Ob River basin. Over the entire watershed, the mean extent of inundation during the snow-free months is 2.6 x 10(5) km(2), consistent with previous independent static or satellites-derived estimates. The maximum in yearly inundation, showing propagation from south to north between April and June, exhibits strong seasonal and inter-annual variations. The consistency of the inundation estimates is then analyzed at local or basin-wide scale using different in situ or satellite-derived snow and runoff parameters. The results show a strong relationship between the inundation extent and the snowmelt date, the snowpack depth at three in situ stations located in the southern part of the basin. Over the northern part, results show that flooding is more closely linked to the amount of water coming downstream from the southern part of the basin. A close systematic relationship is also found between the inundation extent and the local in situ runoff at six locations as well as with the altimeter-derived discharge measured at the Ob estuary. This case study evaluation shows the potential of these data sets to provide consistent information about the seasonal and inter-annual variations of inundation over a major Boreal river basin. These results also suggest new potential to improve the description of the snow-inundation-runoff relationship that are fundamental for climate and hydrological models. C1 Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Observ Paris, Lab Etudes Rayonnement & Matiere Astrophys, CNRS, Paris, France. NOAA, Cooperat Remote Sensing Sci & Technol Ctr, City Coll New York, New York, NY USA. RP Papa, F (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM fpapa@giss.nasa.gov RI Papa, Fabrice/D-3695-2009; Rossow, William/F-3138-2015 OI Papa, Fabrice/0000-0001-6305-6253; NR 32 TC 24 Z9 26 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 22 PY 2007 VL 112 IS D18 AR D18103 DI 10.1029/2007JD008451 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 213RW UT WOS:000249685800001 ER PT J AU Sarzi, M Allard, EL Knapen, JH Mazzuca, LM AF Sarzi, M. Allard, E. L. Knapen, J. H. Mazzuca, L. M. TI Star formation and stellar populations across nuclear rings in galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE HII regions; galaxies : ISM; galaxies : nuclei; galaxies : spiral; galaxies : star clusters; galaxies : stellar content ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; WOLF-RAYET GALAXIES; DISK GALAXIES; SPIRAL GALAXIES; BARRED GALAXIES; HIGH-RESOLUTION; SAURON PROJECT; HOST GALAXIES; INFRARED-SPECTROSCOPY AB We present a study of the optical spectra of a sample of eight star-forming nuclear rings and the nuclei of their host galaxies. The spectra were obtained with the Intermediate dispersion Spectrograph and Imaging System spectrograph on the William Herschel Telescope and cover a wide range in wavelength, enabling the measurement of several stellar absorption features and gas emission lines. We compared the strength of the absorption lines to a variety of population synthesis models for the star formation history in the nuclear rings, including also the contribution of the older bulge and disc stellar components. In agreement with our previous investigation of the nuclear ring of NGC 4321, which was based on a more restricted number of line-strength indices, we find that the stars in our sample of nuclearrings have most likely formed over a prolonged period of time characterized by episodic bursts of star formation activity. Constant star formation is firmly ruledoutby the present data, whereas a one-off formation event is an unlikely explanation for a common galactic component such as nuclear rings. The nuclear rings of NGC 4314 and NGC 7217 have distinct line-strength properties that set them apart from the rest of our sample, which are due to a larger contribution of bulge star in the observed spectra and, in the case of NGC 4314, to a younger stellar population in the ring. We have used emission-line measurements to constrain the physical conditions of the ionized gas within the rings, using the ratio of the [S II]lambda lambda 6716, 6731 lines to estimate the density of the gas, and photoionization model grids within specific diagnostic diagrams to derive metallicity. We find that emission in all nuclear rings originates from H it regions with electron densities typical for these kinds of objects, and that the rings are characterized by values for the gas metallicity ranging from slightly below tojust above solar. We have also studied the spectra of the nuclei of our sample galaxies, all of which display emission lines. Consistent with previous studies for the nuclear activity and stellar populations, the majority of our nuclei appear to be dominated by old stellar populations and by Low-Ionization Nuclear Emission Region like emission. As 20 per cent of nearby spiral galaxies host nuclear rings that are presently forming massive stars, our finding of an episodic star formation history in nuclear rings implies that a significant population remains to be identified of young nuclear rings that are not presently in a massive star formation phase. Nuclear rings may thus be a much more common galactic component than presently known. C1 Univ Hertfordshire, Coll Lane, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sarzi, M (reprint author), Univ Hertfordshire, Coll Lane, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. EM m.sarzi@herts.ac.uk NR 97 TC 39 Z9 39 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2007 VL 380 IS 3 BP 949 EP 962 DI 10.1111/j.1365-2966.2007.12177.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 215YM UT WOS:000249844900007 ER PT J AU Schady, P De Pasquale, M Page, MJ Vetere, L Pandey, SB Wang, XY Cummings, J Zhang, B Zane, S Breeveld, A Burrows, DN Gehrels, N Gronwall, C Hunsberger, S Markwardt, C Mason, KO Meszaros, P Norris, JP Oates, SR Pagani, C Poole, TS Roming, PWA Smith, PJ Vanden Berk, DE AF Schady, P. De Pasquale, M. Page, M. J. Vetere, L. Pandey, S. B. Wang, X. Y. Cummings, J. Zhang, B. Zane, S. Breeveld, A. Burrows, D. N. Gehrels, N. Gronwall, C. Hunsberger, S. Markwardt, C. Mason, K. O. Meszaros, P. Norris, J. P. Oates, S. R. Pagani, C. Poole, T. S. Roming, P. W. A. Smith, P. J. Vanden Berk, D. E. TI Extreme properties of GRB 061007: a highly energetic or a highly collimated burst? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM : jets and outflows; gamma-rays : bursts; gamma-rays : observations ID GAMMA-RAY BURST; AFTERGLOW LIGHT CURVES; POSSIBLE EXPLANATION; DENSE MEDIUM; GRB 990123; SWIFT; EMISSION; LONG; TELESCOPE; DUST AB GRB 061007 was the brightest gamma-ray burst (GRB) to be detected by Swift and was accompanied by an exceptionally luminous afterglow that had a V-band magnitude < 11. 1 at 80 s after the prompt emission. From the start of the Swift observations the afterglow decayed as a power law with a slope of a(x) = 1.66 +/- 0.01 in the X-ray and a(opt), = 1.64 +/- 0.01 in the UV/optical, up to the point that it was no longer detected above background in the optical or X-ray bands. The brightness of this GRB and the similarity in the decay rate of the X-ray, optical and gamma-ray emission from 100s after the trigger distinguish this burst from others and present a challenge to the fireball model. The lack of a cooling or jet break in the afterglow Up to similar to 10(5) s constrains any model that can produce the large luminosity observed in GRB 061007, which we found to require either an excessively large kinetic energy or highly collimated outflow. Analysis of the multiwavelength spectral and high-resolution temporal data taken with Swift suggests an early time jet break to be a more plausible scenario than a highly energetic GRB. This must have occurred within 80 s of the prompt emission, which places an upper limit on the jet opening angle of theta(j) = 0.8 degrees. Such a highly collimated outflow resolves the energy budget problem presented in a spherical emission model, reducin the isotropic-equivalent energy of this burst to E(gamma)(corr) = 10(50) erg, consistent with other GRBs. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Particle Phys & Astron Res Council, Swindon SN2 1SZ, Wilts, England. Penn State Univ, Dept Phys, University Pk, PA 16802 USA. Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. Stanford Univ, Stanford, CA 94305 USA. RP Schady, P (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM ps@mssl.ucl.ac.uk RI Gehrels, Neil/D-2971-2012 NR 75 TC 43 Z9 43 U1 1 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2007 VL 380 IS 3 BP 1041 EP 1052 DI 10.1111/j.1365-2966.2007.12138.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 215YM UT WOS:000249844900016 ER PT J AU Cherng, M Jun, I Jordan, T AF Cherng, M. Jun, I. Jordan, T. TI Optimum shielding in Jovian radiation environment SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 10th International Symposium on Radiation Physics CY SEP 17-22, 2006 CL Univ Coimbra, Coimbra, PORTUGAL HO Univ Coimbra DE Jupiter; Jovian; radiation; shielding; NOVICE; MCNPX AB At Jupiter, the most dominant particle constituent is the high-energy electrons with E> 1 MeV (and can be as high as > 100 MeV). Huge mass is required to shield these electrons to reduce the radiation doses to the acceptable level for spacecraft electronics. An adjoint Monte Carlo code, NOVICE, which was developed specifically for space radiation transport problems, was used as a primary tool to study an optimum shielding design for a Jupiter mission. Also, a traditional forward Monte Carlo code, MCNPX, was used to verify the NOVICE results. Here we studied two representative spacecraft-shielding materials: aluminum representing low/medium-Z material and tungsten representing high-Z material. A series of NOVICE and MCNPX runs were performed to compute the energy deposition in spherical shell geometry with a small silicon detector at the center of the sphere. Calculation results indicate that, for the radiation attenuation required for typical electronics used in a Jupiter mission, the low-Z material and the low/high-Z combination are a less-efficient shield per the same area mass than the high-Z material in the Jovian radiation environment studied here. When massive shielding > 10 g/cm(2) is required to protect very radiation- sensitive electronics, then the low- /high-Z combination is a better shield per the same areal mass. (C) 2007 Elsevier B.V. All rights reserved. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. EMPC, Gaithersburg, MD 20885 USA. RP Cherng, M (reprint author), CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michael.j.cherng@jpl.nasa.gov NR 5 TC 1 Z9 1 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD SEP 21 PY 2007 VL 580 IS 1 BP 633 EP 636 DI 10.1016/j.nima.2007.05.028 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 214MF UT WOS:000249741300162 ER PT J AU McEwen, AS Hansen, CJ Delamere, WA Eliason, EM Herkenhoff, KE Keszthelyi, L Gulick, VC Kirk, RL Mellon, MT Grant, JA Thomas, N Weitz, CM Squyres, SW Bridges, NT Murchie, SL Seelos, F Seelos, K Okubo, CH Milazzo, MP Tornabene, LL Jaeger, WL Byrne, S Russell, PS Griffes, JL Martinez-Alonso, S Davatzes, A Chuang, FC Thomson, BJ Fishbaugh, KE Dundas, CM Kolb, KJ Banks, ME Wray, JJ AF McEwen, A. S. Hansen, C. J. Delamere, W. A. Eliason, E. M. Herkenhoff, K. E. Keszthelyi, L. Gulick, V. C. Kirk, R. L. Mellon, M. T. Grant, J. A. Thomas, N. Weitz, C. M. Squyres, S. W. Bridges, N. T. Murchie, S. L. Seelos, F. Seelos, K. Okubo, C. H. Milazzo, M. P. Tornabene, L. L. Jaeger, W. L. Byrne, S. Russell, P. S. Griffes, J. L. Martinez-Alonso, S. Davatzes, A. Chuang, F. C. Thomson, B. J. Fishbaugh, K. E. Dundas, C. M. Kolb, K. J. Banks, M. E. Wray, J. J. TI A closer look at water-related geologic activity on Mars SO SCIENCE LA English DT Article ID CRATERING RATE; DEPOSITS; MISSION; FATE AB Water has supposedly marked the surface of Mars and produced characteristic landforms. To understand the history of water on Mars, we take a close look at key locations with the High-Resolution Imaging Science Experiment on board the Mars Reconnaissance Orbiter, reaching fine spatial scales of 25 to 32 centimeters per pixel. Boulders ranging up to similar to 2 meters in diameter are ubiquitous in the middle to high latitudes, which include deposits previously interpreted as fine-grained ocean sediments or dusty snow. Bright gully deposits identify six locations with very recent activity, but these lie on steep (20 degrees to 35 degrees) slopes where dry mass wasting could occur. Thus, we cannot confirm the reality of ancient oceans or water in active gullies but do see evidence of fluvial modification of geologically recent mid-latitude gullies and equatorial impact craters. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Delamere Support Syst, Boulder, CO 80304 USA. US Geol Survey, Flagstaff, AZ 86001 USA. NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. Univ Colorado, Boulder, CO 80309 USA. Smithsonian Ctr Earth & Planetary Studies, Washington, DC USA. Planetary Sci Inst, Tucson, AZ 85719 USA. Cornell Univ, Ithaca, NY 14853 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Int Space Sci Inst, Bern, Switzerland. RP McEwen, AS (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM mcewen@lpl.arizona.edu RI Wray, James/B-8457-2008; Davatzes, Alexandra/B-1479-2012; Byrne, Shane/B-8104-2012; Martinez-Alonso, Sara/D-8594-2011; Murchie, Scott/E-8030-2015; Seelos, Kimberly/F-4647-2015; Mellon, Michael/C-3456-2016; Seelos, Frank/C-7875-2016; Bridges, Nathan/D-6341-2016; OI Thomson, Bradley/0000-0001-8635-8932; Wray, James/0000-0001-5559-2179; Martinez-Alonso, Sara/0000-0001-5185-8670; Murchie, Scott/0000-0002-1616-8751; Seelos, Kimberly/0000-0001-7236-0580; Seelos, Frank/0000-0001-9721-941X; Dundas, Colin/0000-0003-2343-7224 NR 23 TC 99 Z9 100 U1 2 U2 22 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 SEP 21 PY 2007 VL 317 IS 5845 BP 1706 EP 1709 DI 10.1126/science.1143987 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 212HD UT WOS:000249585900034 PM 17885125 ER PT J AU Seu, R Phillips, RJ Alberti, G Biccari, D Bonaventura, F Bortone, M Calabrese, D Campbell, BA Cartacci, M Carter, LM Catallo, C Croce, A Croci, R Cutigni, M Di Placido, A Dinardo, S Federico, C Flamini, E Fois, F Frigeri, A Fuga, O Giacomoni, E Gim, YY Guelfi, M Holt, JW Kofman, W Leuschen, CJ Marinangeli, L Marras, P Masdea, A Mattei, S Mecozzi, R Milkovich, SM Morlupi, A Mouginot, J Orosei, R Papa, C Paterno, T del Marmo, PP Pettinelli, E Pica, G Picardi, G Plaut, JJ Provenziani, M Putzig, NE Russo, F Safaeinili, A Salzillo, G Santovito, MR Smrekar, SE Tattarletti, B Vicari, D AF Seu, Roberto Phillips, Roger J. Alberti, Giovanni Biccari, Daniela Bonaventura, Francesco Bortone, Marco Calabrese, Diego Campbell, Bruce A. Cartacci, Marco Carter, Lynn M. Catallo, Claudio Croce, Anna Croci, Renato Cutigni, Marco Di Placido, Antonio Dinardo, Salvatore Federico, Costanzo Flamini, Enrico Fois, Franco Frigeri, Alessandro Fuga, Oreste Giacomoni, Emanuele Gim, Yonggyu Guelfi, Mauro Holt, John W. Kofman, Wlodek Leuschen, Carlton J. Marinangeli, Lucia Marras, Paolo Masdea, Arturo Mattei, Stefania Mecozzi, Riccardo Milkovich, Sarah M. Morlupi, Antonio Mouginot, Jeremie Orosei, Roberto Papa, Claudio Paterno, Tobia del Marmo, Paolo Persi Pettinelli, Elena Pica, Giulia Picardi, Giovanni Plaut, Jeffrey J. Provenziani, Marco Putzig, Nathaniel E. Russo, Federica Safaeinili, Ali Salzillo, Giuseppe Santovito, Maria Rosaria Smrekar, Suzanne E. Tattarletti, Barbara Vicari, Danilo TI Accumulation and erosion of Mars' south polar layered deposits SO SCIENCE LA English DT Article ID RADAR; SUBSURFACE; TOPOGRAPHY; FEATURES; MISSION; HISTORY; CAP AB Mars' polar regions are covered with ice-rich layered deposits that potentially contain a record of climate variations. The sounding radar SHARAD on the Mars Reconnaissance Orbiter mapped detailed subsurface stratigraphy in the Promethei Lingula region of the south polar plateau, Planum Australe. Radar reflections interpreted as layers are correlated across adjacent orbits and are continuous for up to 150 kilometers along spacecraft orbital tracks. The reflectors are often separated into discrete reflector sequences, and strong echoes are seen as deep as 1 kilometer. In some cases, the sequences are dipping with respect to each other, suggesting an interdepositional period of erosion. In Australe Sulci, layers are exhumed, indicating recent erosion. C1 Univ Roma La Sapienza, Dept Info Com, I-00184 Rome, Italy. Washington Univ, St Louis, MO 63130 USA. Consorzio Ric Sistemi Telesensori, I-80125 Naples, Italy. Thales Alenia Space Italia, I-00131 Rome, Italy. Smithsonian Inst, Washington, DC 20013 USA. Univ Perugia, I-06123 Perugia, Italy. Agenzia Spaziale Italiana, I-00198 Rome, Italy. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Texas, Austin, TX 78758 USA. CNRS, F-38041 Grenoble, France. Univ Grenoble 1, F-38041 Grenoble, France. Univ Kansas, Lawrence, KS 66045 USA. Int Res Sch Planetary Sci, I-65127 Pescara, Italy. Ist Nazl Astrofis, I-00133 Rome, Italy. Univ Roma Tre, I-00146 Rome, Italy. RP Seu, R (reprint author), Univ Roma La Sapienza, Dept Info Com, I-00184 Rome, Italy. EM roberto.seu@uniroma1.it RI Kofman, Wlodek/C-4556-2008; Holt, John/C-4896-2009; Frigeri, Alessandro/F-2151-2010; Carter, Lynn/D-2937-2012; Mouginot, Jeremie/G-7045-2015; OI Frigeri, Alessandro/0000-0002-9140-3977; Cartacci, Marco/0000-0001-9825-1817; PETTINELLI, Elena/0000-0002-7066-6516 NR 26 TC 41 Z9 41 U1 2 U2 12 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 21 PY 2007 VL 317 IS 5845 BP 1715 EP 1718 DI 10.1126/science.1144120 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 212HD UT WOS:000249585900037 PM 17885128 ER PT J AU Zuber, MT Phillips, RJ Andrews-Hanna, JC Asmar, SW Konopliv, AS Lemoine, FG Plaut, JJ Smith, DE Smrekar, SE AF Zuber, Maria T. Phillips, Roger J. Andrews-Hanna, Jeffrey C. Asmar, Sami W. Konopliv, Alexander S. Lemoine, Frank G. Plaut, Jeffrey J. Smith, David E. Smrekar, Suzanne E. TI Density of Mars' south polar layered deposits SO SCIENCE LA English DT Article ID CAP AB Both poles of Mars are hidden beneath caps of layered ice. We calculated the density of the south polar layered deposits by combining the gravity field obtained from initial results of radio tracking of the Mars Reconnaissance Orbiter with existing surface topography from the Mars Orbiter Laser Altimeter on the Mars Global Surveyor spacecraft and basal topography from the Mars Advanced Radar for Subsurface and Ionospheric Sounding on the Mars Express spacecraft. The results indicate a best-fit density of 1220 kilograms per cubic meter, which is consistent with water ice that has similar to 15% admixed dust. The results demonstrate that the deposits are probably composed of relatively clean water ice and also refine the martian surface-water inventory. C1 MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. NASA, Goddard Space Flight Ctr, Solar syst Explorat div, Greenbelt, MD 20771 USA. RP Zuber, MT (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM zuber@mit.edu RI Lemoine, Frank/D-1215-2013 NR 15 TC 32 Z9 32 U1 1 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 21 PY 2007 VL 317 IS 5845 BP 1718 EP 1719 DI 10.1126/science.1146995 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 212HD UT WOS:000249585900038 PM 17885129 ER PT J AU Sandford, SA Brownlee, DE AF Sandford, Scott A. Brownlee, Donald E. TI Response to comment on "Organics captured from Comet 81P/Wild 2 by the Stardust spacecraft" SO SCIENCE LA English DT Editorial Material ID SAMPLES C1 NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Sandford, SA (reprint author), NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. EM ssandford@mail.arc.nasa.gov NR 6 TC 3 Z9 3 U1 0 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 21 PY 2007 VL 317 IS 5845 DI 10.1126/science.1145013 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 212HD UT WOS:000249585900022 ER PT J AU Woo, R AF Woo, Richard TI Space weather and deep space communications SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID CORONAL MASS EJECTIONS; DOPPLER SCINTILLATION MEASUREMENTS; RADIO SCATTERING OBSERVATIONS; COLUMNAR CONTENT MEASUREMENTS; HELIOSPHERIC CURRENT SHEET; SOLAR-WIND TURBULENCE; DENSITY-FLUCTUATIONS; INTERPLANETARY DISTURBANCES; FILAMENTARY STRUCTURES; MAGNETIC-FIELDS AB While Pioneer 11 and Galileo are two deep space missions that experienced radio communication disruptions due to space weather, the success of a mission like Solar Probe, whose goal is to fly by the Sun within a few solar radii of its surface, may depend critically on space weather. It is therefore crucial to thoroughly understand how space weather affects radio communications and to identify ways to predict it. In this study, we explain how enhanced small-scale electron density variations in the solar corona represent adverse space weather to radio communications because they give rise to enhancements in radio propagation phenomena such as spectral broadening and fluctuations in intensity and Doppler of the radio signal known as scintillation. The inability of narrowband radio receivers to track the broadened and rapidly fluctuating radio signal leads to disruption in communication and loss of telemetry. Recent advances have been made in understanding enhanced small-scale density variations and their relationship to the Sun, and we show how this makes it possible to use daily observations of unprecedented solar missions like the Solar and Heliospheric Observatory (SOHO) or Solar Terrestrial Relations Observatory (STEREO) to diagnose, monitor, and forecast adverse space weather for deep space communications. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Woo, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM richard.woo@jpl.nasa.gov NR 55 TC 1 Z9 1 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD SEP 21 PY 2007 VL 5 IS 9 AR S09004 DI 10.1029/2006SW000307 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 261JS UT WOS:000253075500001 ER PT J AU Eplee, RE Patt, FS Franz, BA Bailey, SW Meister, G McClain, CR AF Eplee, Robert E., Jr. Patt, Frederick S. Franz, Bryan A. Bailey, Sean W. Meister, Gerhard McClain, Charles R. TI SeaWiFS on-orbit gain and detector calibrations: effect on ocean products SO APPLIED OPTICS LA English DT Article AB The NASA Ocean Biology Processing Group's Calibration and Validation Team has analyzed the mission-long Sea-Viewing Wide Field-of-View Sensor (SeaWiFS) on-orbit gain and detector calibration time series to verify that lunar calibrations, obtained at nonstandard gains and radiance ranges, are valid for Earth data collected at standard gains and typical ocean, cloud, and land radiances. For gain calibrations, a constant voltage injected into the postdetector electronics allows gain ratios to be computed for all four detectors in each band. The on-orbit lunar gain ratio time series show small drifts for the near infrared bands. These drifts are propagated into the ocean color data through the atmospheric correction parameter e, which uses the 765/865 nm band ratio. An anomaly analysis of global mean normalized water-leaving radiances at 510 nm shows a small decrease over the mission, while an analysis of a shows a corresponding increase. The drifts in the lunar time series for the 765 and 865 nm bands were corrected. An analysis of the revised water-leaving radiances at 510 nm shows the drift has been eliminated, while an analysis of a shows a reduced drift. For detector calibrations, solar diffuser observations made by the individual detectors in each band allows the response of the detectors to be monitored separately. The mission-long time series of detector calibration data show that the variations in the response of the individual detectors are less than 0.5% over the mission for all bands except the 865 nm band, where the variations are less than 1%. (C) 2007 Optical Society of America. C1 Sci Applicat Int Corp, Beltsville, MD 20705 USA. Futuretech Corp, Greenbelt, MD 20770 USA. NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA. RP Eplee, RE (reprint author), Sci Applicat Int Corp, 4600 Powder Mill Rd,Suite 400, Beltsville, MD 20705 USA. EM Robert.E.Eplee@nasa.gov RI Franz, Bryan/D-6284-2012; Meister, Gerhard/F-7159-2012; Bailey, Sean/D-3077-2017 OI Franz, Bryan/0000-0003-0293-2082; Bailey, Sean/0000-0001-8339-9763 NR 19 TC 6 Z9 6 U1 0 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD SEP 20 PY 2007 VL 46 IS 27 BP 6733 EP 6750 DI 10.1364/AO.46.006733 PG 18 WC Optics SC Optics GA 224PC UT WOS:000250457900009 PM 17882294 ER PT J AU Odegard, N Arendt, RG Dwek, E Haffner, LM Hauser, MG Reynolds, RJ AF Odegard, N. Arendt, R. G. Dwek, E. Haffner, L. M. Hauser, M. G. Reynolds, R. J. TI Determination of the far-infrared cosmic background using COBE dirbe and wham data SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; diffuse radiation; Galaxy : general; infrared : ISM; ISM : general ID WARM IONIZED MEDIUM; HIGH GALACTIC LATITUDE; H-ALPHA; EXPERIMENT SEARCH; MILKY-WAY; PHYSICAL CONDITIONS; MOLECULAR GAS; DUST EMISSION; SKY SURVEY; CLOUDS AB Determination of the cosmic infrared background (CIB) at far-infrared wavelengths using COBE DIRBE data is limited by the accuracy to which foreground interplanetary and Galactic dust emission can be modeled and subtracted. Most previous determinations of the far-infrared CIB were based on the detection of residual isotropic emission in sky maps from which the emission from interplanetary dust and the neutral interstellar medium were removed. In this paper we use the Wisconsin H alpha Mapper (WHAM) Northern Sky Survey as a tracer of the ionized medium to examine the effect of this foreground component on determination of the CIB. We decompose DIRBE far-infrared data for five high Galactic latitude regions into H-I -and H alpha-correlated components and a residual component. We find the H alpha-correlated component to be consistent with zero for each region, yielding CIB results that are essentially the same as those previously derived by the COBE DIRBE team: nu I-nu(nW m(-2) sr(-1)) < 75, < 32, = 25 +/- 8, and = 13 +/- 3 at 60, 100, 140, and 240 mu m, respectively (upper limits are 2 sigma). For comparison, the estimated integrated light from galaxies based on Spitzer 160 mu m source counts is 13.7 +/- 1.7 and 10.7 +/- 1.4 n Wm(-2) sr(-1) at 140 and 240 mu m, respectively. We derive upper limits on the 100 mu m memissivity of the ionized medium that are typically about 40% of the 100 mu m emissivity of the neutral atomic medium. If H alpha is not a reliable tracer of far-infrared emission, we show that our analysis would underestimate the emissivity of the ionized medium and could slightly overestimate the CIB. C1 ADNET Syst Inc, Rockville, MD USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Odegard, N (reprint author), ADNET Syst Inc, Rockville, MD USA. EM nils.p.odegard@nasa.gov RI Dwek, Eli/C-3995-2012; OI Arendt, Richard/0000-0001-8403-8548; Haffner, Lawrence/0000-0002-9947-6396 NR 61 TC 9 Z9 9 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP 11 EP 25 DI 10.1086/520079 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210KU UT WOS:000249455900002 ER PT J AU Gavazzi, R Treu, T Rhodes, JD Koopmans, LVE Bolton, AS Burles, S Massey, RJ Moustakas, LA AF Gavazzi, Raphael Treu, Tommaso Rhodes, Jason D. Koopmans, Leon V. E. Bolton, Adam S. Burles, Scott Massey, Richard J. Moustakas, Leonidas A. TI The Sloan Lens ACS survey. IV. The mass density profile of early-type galaxies out to 100 effective radii SO ASTROPHYSICAL JOURNAL LA English DT Review DE dark matter; galaxies : elliptical and lenticular, cD; galaxies : structure; gravitational lensing ID DARK-MATTER HALOS; DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; TO-LIGHT RATIOS; LINE-OF-SIGHT; ELLIPTIC GALAXIES; FUNDAMENTAL PLANE; STELLAR MASS; INTERMEDIATE-REDSHIFT; DOMINATED GALAXIES AB We present a weak-lensing analysis of 22 early-type (strong) lens galaxies, based on deep HST images obtained as part of the Sloan Lens ACS Survey. Using advanced techniques to control systematic uncertainties, we show that weak-lensing signal is detected out to similar to 300 h(-1) kpc (at the mean lens redshift z = 0.2). We analyze blank control fields from COSMOS in the same manner, inferring that the residual systematic uncertainty in the tangential shear is less than 0.3%. A joint strong- and weak-lensing analysis shows that the average total mass density profile is consistent with isothermal (i.e., rho proportional to r(-2)) over two decades in radius (3-300 h(-1) kpc, approximately 1-100 effective radii). This finding extends by over an order of magnitude in radius previous results, based on strong lensing and/or stellar dynamics, that luminous and dark components "conspire" to form an isothermal mass distribution. In order to disentangle the contributions of luminous and dark matter, we fit a two-component mass model (deVaucouleurs+NFW) to the weak- and strong-lensing constraints. It provides a good fit to the datawith only two free parameters: (1) the average stellar mass-to-light ratio M-*/L-V =4.48 +/- 0.46 h M-circle dot L-circle dot(-1) (at z = 0.2), in agreement with that expected for an old stellar population; (2) the average virialmass-to-light ratio M-vir/L-V = 246(-87)(+101) h M-circle dot L-circle dot(-1) Taking into account the scatter in the mass-luminosity relation, the latter result is in good agreement with semianalytical models of massive galaxy formation. The dark matter fraction inside the sphere of radius, the effective radius, is found to be 27% +/- 4%. Our results are consistent with galaxy-galaxy lensing studies of early-type galaxies that are not strong lenses, in the 30- 300 h(-1) kpc radius range. Thus, within the uncertainties, our results are representative of early- type galaxies in general. C1 Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Pasadena, CA 91125 USA. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Gavazzi, R (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. OI Moustakas, Leonidas/0000-0003-3030-2360 NR 107 TC 231 Z9 232 U1 0 U2 7 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 SEP 20 PY 2007 VL 667 IS 1 BP 176 EP 190 DI 10.1086/519237 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210KU UT WOS:000249455900015 ER PT J AU Chapman, NL Lai, SP Mundy, LG Evans, NJ Brooke, TY Cieza, LA Spiesman, WJ Rebull, LM Stapelfeldt, KR Noriega-Crespo, A Lanz, L Allen, LE Blake, GA Bourke, TL Harvey, PM Huard, TL Jorgensen, JK Koerner, DW Myers, PC Padgett, DL Sargent, AI Teuben, P van Dishoeck, EF Wahhaj, Z Young, KE AF Chapman, Nicholas L. Lai, Shih-Ping Mundy, Lee G. Evans, Neal J., II Brooke, Timothy Y. Cieza, Lucas A. Spiesman, William J. Rebull, Luisa M. Stapelfeldt, Karl R. Noriega-Crespo, Alberto Lanz, Lauranne Allen, Lori E. Blake, Geoffrey A. Bourke, Tyler L. Harvey, Paul M. Huard, Tracy L. Jorgensen, Jes K. Koerner, David W. Myers, Philip C. Padgett, Deborah L. Sargent, Annelia I. Teuben, Peter van Dishoeck, Ewine F. Wahhaj, Zahed Young, Kaisa E. TI The Spitzer c2d survey of large, nearby, interstellar clouds. IV. Lupus observed with mips SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : clouds; stars : formation ID MAIN-SEQUENCE STARS; LOW-MASS MEMBERS; SPACE-TELESCOPE; STELLAR POPULATION; J=1-0 OBSERVATIONS; MOLECULAR CLOUDS; DARK CLOUD; DUST; EXTINCTION; IRAC AB We present maps of 7.78 deg(2) of the Lupus molecular cloud complex at 24, 70, and 160 mu m. They were made with the Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS) instrument as part of the Spitzer Legacy Program "From Molecular Cores to Planet-Forming Disks" (c2d). The maps cover three separate regions in Lupus, denoted I, III, and IV. We discuss the c2d pipeline and how our data processing differs from it. We compare source counts in the three regions with two other data sets and predicted star counts from the Wainscoat model. This comparison shows the contribution from background galaxies in Lupus I. We also create two color-magnitude diagrams using the 2MASS and MIPS data. From these results, we can identify background galaxies and distinguish them from probable young stellar objects. The sources in our catalogs are classified based on their spectral energy distribution ( SED) from 2MASS and Spitzer wavelengths to create a sample of young stellar object candidates. From 2MASS data, we create extinction maps for each region and note a strong correspondence between the extinction and the 160 mu m emission. The masses we derived in each Lupus cloud from our extinction maps are compared to masses estimated from (CO)-C-13 and C-18 O and found to be similar to our extinction masses in some regions, but significantly different in others. Finally, based on our color-magnitude diagrams, we selected 12 of our reddest candidate young stellar objects for individual discussion. Five of the 12 appear to be newly discovered YSOs. C1 Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Natl Tsing Hua Univ, Inst Astron, Hsinchu 30043, Taiwan. Natl Tsing Hua Univ, Dept Phys, Hsinchu 30043, Taiwan. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Univ Texas, Dept Astron, Austin, TX 78712 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. Inst Astron, Honolulu, HI 96822 USA. Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70301 USA. RP Chapman, NL (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM chapman@astro.umd.edu RI Stapelfeldt, Karl/D-2721-2012; OI Lanz, Lauranne/0000-0002-3249-8224; Rebull, Luisa/0000-0001-6381-515X NR 51 TC 25 Z9 25 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP 288 EP 302 DI 10.1086/520790 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210KU UT WOS:000249455900024 ER PT J AU Cieza, L Padgett, DL Stapelfeldt, KR Augereau, JC Harvey, P Evans, NJ Merin, B Koerner, D Sargent, A van Dishoeck, EF Allen, L Blake, G Brooke, T Chapman, N Huard, T Lai, SP Mundy, L Myers, PC Spiesman, W Wahhaj, Z AF Cieza, Lucas Padgett, Deborah L. Stapelfeldt, Karl R. Augereau, Jean-Charles Harvey, Paul Evans, Neal J., II Merin, Bruno Koerner, David Sargent, Anneila van Dishoeck, Ewine F. Allen, Lori Blake, Geoffrey Brooke, Timothy Chapman, Nicholas Huard, Tracy Lai, Shih-Ping Mundy, Lee Myers, Philip C. Spiesman, William Wahhaj, Zahed TI The Spitzer c2d survey of weak-line T Tauri stars. II. New constraints on the timescale for planet building SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; open clusters and associations : individual (IC 348) planetary systems : protoplanetary disks; stars : pre-main-sequence ID MAIN-SEQUENCE STARS; LOW-MASS STARS; SUN-LIKE STARS; ALL-SKY SURVEY; YOUNG STARS; PROTOPLANETARY DISKS; FORMING REGION; OB ASSOCIATION; DEBRIS DISKS; INTERSTELLAR CLOUDS AB One of the central goals of the Spitzer Legacy Project "From Cores to Disks'' (c2d) is to determine the frequency of circumstellar disks around weak-line T Tauri stars (WTTSs) and to study the properties and evolutionary status of these disks. Here we present a census of disks for a sample of over 230 WTTSs located in the c2d IRAC and MIPS maps of the Ophiuchus, Lupus, and Perseus Molecular Clouds. We find that similar to 20% of the WTTSs in a magnitude-limited subsample have IR excesses at IRAC wavelengths. These disks frequencies are similar to 3-6 times larger than that recently found for a sample of relatively isolated WTTSs located outside the highest extinction regions covered by the c2d maps. The disk fractions we find are more consistent with those obtained in recent Spitzer studies of WTTSs in young clusters such as IC 348 and Tr37. According to their location in the H-R diagram, the WTTSs with excesses in our sample are among the younger part of the age distribution. Still, up to similar to 50% of the apparently youngest stars in the sample show no evidence of IR excess, suggesting that the circumstellar disks of a sizable fraction of pre-main-sequence stars dissipate in a timescale of similar to 1 Myr. We also find that none of the stars in our sample apparently older than similar to 10 Myr have detectable circumstellar disks at wavelengths < 24 mu m. The WTTS disks in our sample exhibit a wide range of properties (SED morphology, inner radius, L-disk/L-*, etc.) that bridge the gaps observed between the CTTSs and the debris disk regimes. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Lab Astrophys Grenoble, F-38041 Grenoble 9, France. Leiden Observ, NL-2300 RA Leiden, Netherlands. European Space Agcy, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Cieza, L (reprint author), Univ Texas, Dept Astron, Austin, TX 78712 USA. RI Stapelfeldt, Karl/D-2721-2012; OI Merin, Bruno/0000-0002-8555-3012 NR 82 TC 120 Z9 121 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP 308 EP 328 DI 10.1086/520698 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210KU UT WOS:000249455900026 ER PT J AU Titarchuk, L Kuznetsov, S Shaposhnikov, N AF Titarchuk, Lev Kuznetsov, Sergey Shaposhnikov, Nickolai TI Correlations between X-ray spectral and timing characteristics in cygnus X-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (Cygnus X-2, Sco X-1); stars : neutron; X-rays : individual (Cygnus X-2, Sco X-1) ID QUASI-PERIODIC OSCILLATIONS; NEUTRON-STAR; BLACK-HOLE; OBSERVATIONAL EVIDENCE; COMPTONIZATION MODELS; FREQUENCY CORRELATION; MONTE-CARLO; 4U 0614+091; GX 17+2; BINARIES AB Correlations between the quasi-periodic oscillations (QPOs) and the spectral power-law index have been reported for a number of black hole candidate sources and for four neutron star (NS) sources, 4U0614+09, 4U 1608-52, 4U 1728-34, and Sco X-1. An examination of QPO frequencies and index relationship in Cyg X-2 is reported herein. The RXTE spectrum of Cyg X-2 can be adequately represented by a simple two-component model of Compton upscattering with a soft photon electron temperature of about 0.7 keV and an iron K line. Inferred spectral power-law index shows correlation with the low QPO frequencies. We find that the Thomson optical depth of the Compton cloud (CC)tau, in framework of spherical geometry, is in the range of similar to 4-6, which is consistent with the surface of the neutron star (NS) being obscured. The NS high-frequency pulsations are presumably suppressed as a result of photon scattering off CC electrons because of such high values of tau. We also point out a number of similarities in terms of timing (presence of low- and high-frequency QPOs) and spectral (high CC optical depth and low CC plasma temperature) appearances between Cyg X-2 and Sco X-1. C1 George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. NASA, Goddard Space Flight Ctr, USRA, Greenbelt, MD 20771 USA. USN, Res Lab, Washington, DC 20375 USA. Univ Calif Riverside, IGPP, Riverside, CA 92521 USA. Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. RP Titarchuk, L (reprint author), George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. EM Lev.Titarchuk@nrl.navy.mil; nikolai@milkyway.gsfc.nasa.gov NR 38 TC 12 Z9 12 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP 404 EP 410 DI 10.1086/520759 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210KU UT WOS:000249455900035 ER PT J AU Gautier, TN Rieke, GH Stansberry, J Bryden, GC Stapelfeldt, KR Werner, MW Beichman, CA Chen, C Su, K Trilling, D Patten, BM Roellig, TL AF Gautier, Thomas N. Rieke, G. H. Stansberry, John Bryden, Geoffrey C. Stapelfeldt, Karl R. Werner, Michael W. Beichman, Charles A. Chen, Christine Su, Kate Trilling, David Patten, Brian M. Roellig, Thomas L. TI Far-infrared properties of M dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; planetary systems; stars : fundamental parameters (colors); stars : late-type ID MULTIBAND IMAGING PHOTOMETER; MAIN-SEQUENCE; REDUCTION ALGORITHMS; ULTRACOOL DWARFS; DEBRIS DISKS; SPITZER MIPS; T-DWARFS; STARS; NEARBY; NEIGHBORS AB We report the mid- and far-infrared properties of nearby M dwarfs. Spitzer MIPS measurements were obtained for a sample of 62 stars at 24 mu m, with subsamples of 41 and 20 stars observed at 70 and 160 mu m, respectively. We compare the results with current models of M star photospheres and look for indications of circumstellar dust in the form of significant deviations of K-[24 mu m] colors and 70 mu m/24 mu m flux ratios from the average M star values. At 24 mu m, all 62 of the targets were detected; 70 mu m detections were achieved for 20 targets in the subsample observed, and no detections were seen in the 160 mu m subsample. No clear far-infrared excesses were detected in our sample. The average far-infrared excess relative to the photospheric emission of the M stars is at least 4 times smaller than the similar average for a sample of solar-type stars. However, this limit allows the average fractional infrared luminosity in the M-star sample to be similar to that for more massive stars. We have also set low limits (10(-4) to 10(-9) M-circle times depending on location) for the maximum mass of dust possible around our stars. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gautier, TN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM thomas.n.gautier@jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012; OI Su, Kate/0000-0002-3532-5580 NR 38 TC 70 Z9 70 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP 527 EP 536 DI 10.1086/520667 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210KU UT WOS:000249455900046 ER PT J AU Leggett, SK Marley, MS Freedman, R Saumon, D Liu, MC Geballe, TR Golimowski, DA Stephens, DC AF Leggett, S. K. Marley, M. S. Freedman, R. Saumon, D. Liu, Michael C. Geballe, T. R. Golimowski, D. A. Stephens, D. C. TI Physical and spectral characteristics of the T8 and later type dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : individual (2MASS J04151954-0935066, 2MASS J09393548-2448279, 2MASS J11145133-2618235, HD 3651B; G1 570D); stars : low-mass, brown dwarfs ID SPITZER-SPACE-TELESCOPE; ALL-SKY SURVEY; INFRARED SPECTROGRAPH IRS; EXOPLANET HOST STAR; BROWN DWARF; GLIESE 570D; K-DWARF; METHANE; DISCOVERY; 2MASS AB We use newly observed and published near-infrared spectra, together with synthetic spectra obtained from model atmospheres, to derive physical properties of three of the latest type T dwarfs. A new R approximate to 1700 spectrum of the T7.5 dwarf HD 3651B, together with existing data, allows a detailed comparison to the well-studied and very similar dwarf Gl 570D. We find that HD 3651B has both higher gravity and higher metallicity than Gl 570D, with best-fit atmospheric parameters of T-eff 820-830 K, log g = 5.4-5.5, [m/ H] = +0.2, and K-zz 10(4) cm(2) s(-1). Its age is 8-12 Gyr, and its implied mass is 60-70 M-J. We perform a similar analysis of the T8 and T7.5 dwarfs 2MASS J09393548-2448279 and 2MASS J11145133-2618235 using published data, comparing them to the well-studied T8, 2MASS J04151954-0935066. We find that these two dwarfs have effectively the same T-eff as the reference dwarf, and similar or slightly higher gravities, but lower metallicities. The derived parameters are T-eff 725-775 K and [m/H] = -0.3; log g = 5.3 - 5.45 for 2MASS J09393548-2448279 and log g 5.0 - 5.3 for 2MASS J11145133-261823. The age and mass are similar to 10 Gyr and 60 M-J for 2MASS J09393548-2448279, and similar to 5 Gyr and 40 MJ for 2MASS J11145133-261823. A serious limitation to such analyses is the incompleteness of the line lists for transitions of CH4 and NH3 at lambda <= 1.7 mu m, which are also needed for synthesizing the spectrum of the later, cooler, Y type. Spectra of Saturn and Jupiter, and of laboratory CH4 and NH3 gas, suggest that NH3 features in the Y and J bands may be useful as indicators of the next spectral type, and not features in the H and K bands, as previously thought. However, until cooler objects are found, or the line lists improve, large uncertainties remain, as the abundance of NH3 is likely to be significantly below the chemical equilibrium value. Moreover, inclusion of laboratory NH3 opacities in our models predicts band shapes that are discrepant with existing data. It is possible that the T spectral class will have to be extended to temperatures around 400 K, when water clouds condense in the atmosphere and dramatically change the spectral energy distribution of the brown dwarf. C1 Gemini Observ, Hilo, HI 96720 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI, Mountain View, CA 94043 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. RP Leggett, SK (reprint author), Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA. EM dsaumon@lanl.gov OI Leggett, Sandy/0000-0002-3681-2989 NR 68 TC 61 Z9 61 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP 537 EP 548 DI 10.1086/519948 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210KU UT WOS:000249455900047 ER PT J AU Guver, T Ozel, F Gogus, E Kouveliotou, C AF Guever, Tolga Oezel, Feryal Goegues, Ersin Kouveliotou, Chryssa TI The magnetar nature and the outburst mechanism of a transient anomalous X-ray pulsar SO ASTROPHYSICAL JOURNAL LA English DT Article ID XTE J1810-197; XTE-J1810-197; MAGNETOSPHERES; EMISSION; BURSTS AB Anomalous X-ray pulsars ( AXPs) belong to a class of neutron stars believed to harbor the strongest magnetic fields in the universe, as indicated by their energetic bursts and their rapid spin-downs. However, an unambiguous measurement of their surface field strengths has not been made to date. It is also not known whether AXP outbursts result from changes in the neutron star magnetic field or crust properties. Here we report a spectroscopic measurement of the surface magnetic field strength of an AXP, XTE J1810-197, and solidify its magnetar nature. The field strength obtained from detailed spectral analysis and modeling, B = ( 2.72 +/- 0.03) x 10(14) G, is remarkably close to the value inferred from the rate of spin-down of this source and remains nearly constant during numerous observations spanning over an order of magnitude in source flux. The surface temperature, on the other hand, declines steadily and dramatically following the 2003 outburst of this source. Our findings demonstrate that heating occurs in the upper neutron star crust during an outburst and sheds light on the transient behavior of AXPs. C1 Istanbul Univ, Fac Sci, Astron & Space Sci Dept, TR-34119 Istanbul, Turkey. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Guver, T (reprint author), Istanbul Univ, Fac Sci, Astron & Space Sci Dept, TR-34119 Istanbul, Turkey. RI Guver, Tolga/C-1408-2011; Guver, Tolga/B-1039-2014 OI Guver, Tolga/0000-0002-3531-9842 NR 17 TC 41 Z9 41 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP L73 EP L76 DI 10.1086/522047 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210NJ UT WOS:000249462600019 ER PT J AU Huynh, MT Frayer, DT Mobasher, B Dickinson, M Chary, RR Morrison, G AF Huynh, Minh T. Frayer, David T. Mobasher, Bahram Dickinson, Mark Chary, Ranga-Ram Morrison, Glenn TI The far-infrared luminosity function from goods-north: Constraining the evolution of infrared galaxies for z <= 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; infrared : galaxies ID STAR-FORMING GALAXIES; DEEP-FIELD-NORTH; MICRON SOURCE COUNTS; SUBMILLIMETER GALAXIES; REDSHIFT SURVEY; RADIO-SOURCES; SPITZER VIEW; 1.4 GHZ; SAMPLE; HISTORY AB We present the IR luminosity function derived from ultradeep 70 mu m imaging of the GOODS-North field. The 70 mu m observations are longward of the PAH and silicate features which complicate work in the MIR. We derive far-infrared luminosities for the 143 sources with S-70 > 2 mJy (S/N > 3 sigma). The majority (81%) of the sources have spectroscopic redshifts, and photometric redshifts are calculated for the remainder. The IR luminosity function at four redshifts (z similar to 0.28, 0.48, 0.78, and 0.97) is derived and compared to the local one. There is considerable degeneracy between luminosity and density evolution. If the evolving luminosity function is described as rho(L, z) = (1+ z)(q) rho(L/(1 + Z)(p),0), we find q = -2.19p + 6.09. In the case of pure luminosity evolution, we find a best fit of p = 2.78(-0.32)(+0.34). This is consistent with the results from 24 mu m and 1.4 GHz studies. Our results confirm the emerging picture of strong evolution in LIRGs and ULIRGs at 0.4 < z < 1.1 , but we find no evidence of significant evolution in the sub-LIRG (L < 10(11) L-circle dot) population for z < 0.4. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Huynh, MT (reprint author), CALTECH, Spitzer Sci Ctr, MC 220-6, Pasadena, CA 91125 USA. EM mhuynh@ipac.caltech.edu NR 37 TC 25 Z9 25 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP L9 EP L12 DI 10.1086/521981 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210NJ UT WOS:000249462600003 ER PT J AU Stecker, FW Baring, MG Summerlin, EJ AF Stecker, Floyd W. Baring, Matthew G. Summerlin, Errol J. TI Blazar gamma-rays, shock acceleration, and the extragalactic background light SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : general; diffuse radiation; gamma rays : theory ID MONTE-CARLO SIMULATIONS; PARTICLE-ACCELERATION; OBLIQUE SHOCKS; COSMIC-RAYS; RELATIVISTIC SHOCKS; FERMI ACCELERATION; MAGNETIC-FIELDS; STAR-FORMATION; SPITZER VIEW; ENERGY AB The observed spectra of blazars, their intrinsic emission, and the underlying populations of radiating particles are intimately related. The use of these sources as probes of the extragalactic infrared background, a prospect propelled by recent advances in TeV- band telescopes, soon to be augmented by observations by NASA's upcoming Gamma-Ray Large Area Space Telescope, has been a topic of great recent interest. Here, it is demonstrated that if particles in blazar jets are accelerated at relativistic shocks, then gamma-ray spectra with indices less than 1.5 can be produced. This, in turn, loosens the upper limits on the near-infrared extragalactic background radiation previously proposed. We also show evidence hinting that TeV blazars with flatter spectra have higher intrinsic TeV gamma-ray luminosities, and we indicate that there may be a correlation of flatness and luminosity with redshift. C1 NASA, Goddard Space Flight Ctr, Dept Phys & Astron, Greenbelt, MD 20771 USA. Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Dept Phys & Astron, Greenbelt, MD 20771 USA. EM stecker@milkyway.gsfc.nasa.gov; baring@rice.edu; xerex@rice.edu RI Stecker, Floyd/D-3169-2012 NR 38 TC 100 Z9 100 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2007 VL 667 IS 1 BP L29 EP L32 DI 10.1086/522005 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 210NJ UT WOS:000249462600008 ER PT J AU Huang, JP Minnis, P Yi, YH Tang, Q Wang, X Hu, YX Liu, ZY Ayers, K Trepte, C Winker, D AF Huang, Jianping Minnis, Patrick Yi, Yuhong Tang, Qiang Wang, Xin Hu, Yongxiang Liu, Zhaoyan Ayers, Kirk Trepte, Charles Winker, David TI Summer dust aerosols detected from CALIPSO over the Tibetan Plateau SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MINERAL DUST; ASIAN DUST; SAHARAN DUST; EAST-ASIA; CLOUD; LIDAR; EVENTS AB Summertime Tibetan dust aerosol plumes are detected from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite. CALIPSO reveals that dust storms occur more frequently than previously found from Tibetan surface observations because few surface sites were available over remote northwestern Tibet due to high elevation and harsh climate. The Tibetan dust aerosol is characterized by column-averaged volume depolarization and total volume color ratios around 21% and 0.83, respectively. The dust layers appear most frequently around 4-7 km above mean sea level. The volume depolarization ratio for about 90% of the dust particles is less than 10% at low altitudes (3-5 km), while only about 50% of the particles have a greater depolarization ratio at higher altitudes (7-10 km). The 4-day back trajectory analyses show that these plumes probably originate from the nearby Taklamakan desert surface and accumulate over the northern slopes of the Tibetan Plateau. These dust outbreaks can affect the radiation balance of the atmosphere of Tibet because they both absorb and reflect solar radiation. Citation: Huang, J., P. Minnis, Y. Yi, Q. Tang, X. Wang, Y. Hu, Z. Liu, K. Ayers, C. Trepte, and D. Winker ( 2007), Summer dust aerosols detected from CALIPSO over the Tibetan Plateau, Geophys. Res. Lett., 34, L18805, doi: 10.1029/ 2007GL029938. C1 Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. Sci Syst & Applicat Inc, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Inst Aerosp, Hampton, VA 23666 USA. RP Huang, JP (reprint author), Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. EM hjp@lzu.edu.cn RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Minnis, Patrick/G-1902-2010; Hu, Yongxiang/K-4426-2012; wang, xin/H-3936-2015 OI Liu, Zhaoyan/0000-0003-4996-5738; Minnis, Patrick/0000-0002-4733-6148; wang, xin/0000-0002-8839-8345 NR 24 TC 119 Z9 139 U1 7 U2 31 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 20 PY 2007 VL 34 IS 18 AR L18805 DI 10.1029/2007GL029938 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 213RB UT WOS:000249683700001 ER PT J AU Mitrofanov, IG Zuber, MT Litvak, ML Demidov, NE Sanin, AB Boynton, WV Gilichinsky, DA Hamara, D Kozyrev, AS Saunders, RD Smith, DE Tretyakov, VI AF Mitrofanov, I. G. Zuber, M. T. Litvak, M. L. Demidov, N. E. Sanin, A. B. Boynton, W. V. Gilichinsky, D. A. Hamara, D. Kozyrev, A. S. Saunders, R. D. Smith, D. E. Tretyakov, V. I. TI Water ice permafrost on Mars: Layering structure and subsurface distribution according to HEND/Odyssey and MOLA/MGS data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ORBITER LASER ALTIMETER; ODYSSEY; HYDROGEN AB To elucidate the nature of permafrost in the shallow subsurface of Mars, we analyze jointly neutron albedo from the High Energy Neutron Detector (HEND) on the Mars Odyssey spacecraft and near-IR (1064-nm) surface reflectance from the Mars Orbiter Laser Altimeter (MOLA) on Mars Global Surveyor. The first dataset measures the content of hydrogen ( in the form of water or hydroxyl) in the soil, and the second yields the flux of absorbed solar energy by the surface. We identify a statistically-significant negative cross-correlation between these data at latitudes poleward of 40 degrees latitude in the northern hemisphere and in the latitude band 40 degrees - 60 degrees in the southern hemisphere, which we interpret as evidence for the presence of stable water ice under a dry equilibrium top layer (ETL). We deduce an empirical relation between near-IR reflectance and thickness of this ETL, which allows the burial depth of the water ice table to be estimated with km-scale spatial resolution. We observe no correlation between neutron and near-IR albedo within the southern hemisphere poleward of 60 degrees latitude. While it is known from previously analyzed neutron and gamma-ray data that subsurface water ice is present within this region and is covered by a layer of dry regolith, the absence of a correlation indicates that the thickness of this layer is not controlled by an equilibrium condition between the ice table and atmosphere. Citation: Mitrofanov, I. G., et al. ( 2007), Water ice permafrost on Mars: Layering structure and subsurface distribution according to HEND/Odyssey and MOLA/MGS data, Geophys. Res. Lett., 34, L18102, doi: 10.1029/ 2007GL030030. C1 Moscow Space Res Inst, Moscow 117997, Russia. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Inst Phys Chem & Biol Problems Soil Sci, Pushchino 142290, Russia. NASA, Washington, DC 20514 USA. NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Mitrofanov, IG (reprint author), Moscow Space Res Inst, Profsojuznaya St 84-32, Moscow 117997, Russia. EM imitrofa@space.ru NR 13 TC 6 Z9 8 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 20 PY 2007 VL 34 IS 18 AR L18102 DI 10.1029/2007GL030030 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 213RB UT WOS:000249683700002 ER PT J AU Rosenzweig, JB Cook, AM Dunning, M England, RJ Musumeci, P Bellaveglia, M Boscolo, M Catani, L Cianchi, A Di Pirro, G Ferrario, M Fillipetto, D Gatti, G Palumbo, L Serafini, L Vicario, C AF Rosenzweig, J. B. Cook, A. M. Dunning, M. England, R. J. Musumeci, P. Bellaveglia, M. Boscolo, M. Catani, L. Cianchi, A. Di Pirro, G. Ferrario, M. Fillipetto, D. Gatti, G. Palumbo, L. Serafini, L. Vicario, C. TI Experimental testing of dynamically optimized photoelectron beams SO INTERNATIONAL JOURNAL OF MODERN PHYSICS A LA English DT Article; Proceedings Paper CT 46th Workshop on Physics and Applications of High Brightness Electon Beams CY OCT 09-14, 2005 CL Erice, ITALY SP ICFA ID EMITTANCE COMPENSATION AB We discuss the design of and initial results from an experiment in space-charge dominated beam dynamics which explores a new regime of high-brightness electron beam generation at the SPARC (located at INFN-LNF, Frascati) photoinjector. The scheme under study employs the natural tendency in intense electron beams to configure themselves to produce a uniform density, giving a nearly ideal beam from the viewpoint of space charge-induced emittance. The experiments are aimed at testing the marriage of this idea with a related concept, emittance compensation, We show that the existing infrastructure at SPARC is nearly ideal for the proposed tests, and that this new regime of operating photoinjector may be the preferred method of obtaining highest brightness beams with lower energy spread. We discuss the design of the experiment, including developing of a novel time-dependent, aerogel-based imaging system. This system has been installed at SPARC, and first evidence for nearly uniformly filled ellipsoidal charge distributions recorded. C1 [Rosenzweig, J. B.; Cook, A. M.; Dunning, M.; England, R. J.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Bellaveglia, M.; Boscolo, M.; Catani, L.; Cianchi, A.; Di Pirro, G.; Ferrario, M.; Fillipetto, D.; Gatti, G.; Palumbo, L.; Vicario, C.] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, RM, Italy. [Musumeci, P.] Ist Nazl Fis Nucl, Sez Roma 1, Rome, RM, Italy. [Serafini, L.] Ist Nazl Fis Nucl, Sez Milano, I-20133 Milan, MI, Italy. CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. RP Rosenzweig, JB (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, 405 Hilgard Ave, Los Angeles, CA 90095 USA. RI Cianchi, Alessandro/H-1493-2012; Cook, Alan/D-2557-2013; Gatti, Giancarlo/K-3345-2013; Cianchi, Alessandro/A-9581-2016; OI Gatti, Giancarlo/0000-0001-7730-7893; Cianchi, Alessandro/0000-0002-9631-2505; Di Pirro, Giampiero/0000-0002-3004-0754; Boscolo, Manuela/0000-0002-1997-6041 NR 10 TC 1 Z9 1 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-751X J9 INT J MOD PHYS A JI Int. J. Mod. Phys. A PD SEP 20 PY 2007 VL 22 IS 23 BP 4158 EP 4178 DI 10.1142/S0217751X0703772X PG 21 WC Physics, Nuclear; Physics, Particles & Fields SC Physics GA 242GU UT WOS:000251713400014 ER PT J AU Sellers, PJ Fennessy, MJ Dickinson, RE AF Sellers, P. J. Fennessy, M. J. Dickinson, R. E. TI A numerical approach to calculating soil wetness and evapotranspiration over large grid areas SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID HETEROGENEITY; MODELS; FLUX; REPRESENTATION; MOISTURE; SCHEMES; CLIMATE; ENERGY; CARBON; IMPACT AB [1] Soil wetness is typically highly variable in space over the length scales of general circulation model grid areas (similar to 100 km), and the stress functions relating the surface evapotranspiration rate to local-scale (similar to 1-100 m) soil wetness are very nonlinear. These two factors give rise to significant inaccuracies whenever a single grid area average soil wetness value is inserted into a stress function to calculate the evapotranspiration rate for a large grid area. A numerical method is presented to mitigate this problem. The distribution of soil wetness within a grid area is represented by binning, and a numerical integration of the stress function over this binned distribution provides a spatially integrated wetness stress term for the whole grid area, which permits calculation of grid area fluxes in a single operation. The method is very accurate when 10 or more bins are used. It can deal realistically with spatially variable precipitation, conserves moisture exactly, strongly reduces any oscillations, and allows for precise modification of the soil wetness distribution after every time step. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Ctr Ocean Land Atmosphere Studies, Calverton, MD USA. Georgia Inst Technol, Atlanta, GA 30332 USA. RP Sellers, PJ (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 25 TC 6 Z9 6 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 20 PY 2007 VL 112 IS D18 AR D18106 DI 10.1029/2007JD008781 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 213RQ UT WOS:000249685200005 ER PT J AU Thornton, BF Toohey, DW Tuck, AF Elkins, JW Kelly, KK Hovde, SJ Richard, EC Rosenlof, KH Thompson, TL Mahoney, MJ Wilson, JC AF Thornton, Brett F. Toohey, Darin W. Tuck, A. F. Elkins, J. W. Kelly, K. K. Hovde, S. J. Richard, E. C. Rosenlof, K. H. Thompson, T. L. Mahoney, M. J. Wilson, J. C. TI Chlorine activation near the midlatitude tropopause SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID IN-SITU MEASUREMENTS; STRATOSPHERIC OZONE DEPLETION; HEMISPHERE LOWER STRATOSPHERE; HETEROGENEOUS CHEMISTRY; VERTICAL-DISTRIBUTION; CIRRUS CLOUDS; PARTICLE FORMATION; UPPER TROPOSPHERE; SULFATE AEROSOLS; ER-2 AIRCRAFT AB [1] We report on substantial chlorine activation near the midlatitude tropopause over the central United States (39-42 degrees N 102-105 degrees W) during the WB-57F Aerosol Mission (WAM) in April 1998. The extent of activation was determined by simultaneous in situ measurements of ClO and ozone and calculations of total inorganic chlorine (Cl-y) based on recently reported relationships between HCl, ozone, and halocarbons for similar latitudes. Levels of [ClO]/[Cly] approaching 50% occurred in a region of strong gravity wave activity, high particulate surface areas (5-20 mu m 2 cm(-3)), low ozone, and relatively high humidities (20-25 ppm of H2O, yet undersaturated with respect to ice), consistent with a heterogeneous mechanism on particles formed in recently lofted tropospheric air as it mixed into the lowermost stratosphere. These observations are similar to a previous one of chlorine activation on volcanic aerosol, suggesting a common heterogeneous chemical mechanism involving HCl, ClNO3, and HOCl that even in volcanically quiescent years can impact ozone photochemistry in regions of the lowermost stratosphere influenced by mixing from the tropopause region. Models not incorporating this chlorine activation process may be underestimating the impact on ozone in the midlatitude lowermost stratosphere by decomposition of very short lived halocarbon compounds, including substitutes for ozone-depleting compounds. C1 Univ Colorado, Boulder, CO 80309 USA. NOAA, Earth Syst Res Lab, Boulder, CO USA. CALTECH, NASA, Jet Propuls Lab, Pasadena, CA 91125 USA. Univ Denver, Dept Engn, Denver, CO 80208 USA. RP Thornton, BF (reprint author), Univ Colorado, Boulder, CO 80309 USA. RI Toohey, Darin/A-4267-2008; Rosenlof, Karen/B-5652-2008; Tuck, Adrian/F-6024-2011; Manager, CSD Publications/B-2789-2015 OI Toohey, Darin/0000-0003-2853-1068; Rosenlof, Karen/0000-0002-0903-8270; Tuck, Adrian/0000-0002-2074-0538; NR 70 TC 12 Z9 12 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 20 PY 2007 VL 112 IS D18 AR D18306 DI 10.1029/2006JD007640 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 213RQ UT WOS:000249685200001 ER PT J AU Koike, M Kondo, Y Kita, K Takegawa, N Nishi, N Kashihara, T Kawakami, S Kudoh, S Blake, D Shirai, T Liley, B Ko, M Miyazaki, Y Kawasaki, Z Ogawa, T AF Koike, M. Kondo, Y. Kita, K. Takegawa, N. Nishi, N. Kashihara, T. Kawakami, S. Kudoh, S. Blake, D. Shirai, T. Liley, B. Ko, M. Miyazaki, Y. Kawasaki, Z. Ogawa, T. TI Measurements of reactive nitrogen produced by tropical thunderstorms during BIBLE-C SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LIGHTNING-PRODUCED NOX; OPTICAL TRANSIENT DETECTOR; ATLANTIC FLIGHT CORRIDOR; AIRBORNE MEASUREMENTS; UPPER TROPOSPHERE; GLOBAL DISTRIBUTION; UNITED-STATES; STERAO-A; JULY 10; CLOUD AB The Biomass Burning and Lightning Experiment phase C (BIBLE-C) aircraft mission was carried out near Darwin, Australia ( 12 degrees S, 131 degrees E) in December 2000. This was the first aircraft experiment designed to estimate lightning NO production rates in the tropics, where production is considered to be most intense. During the two flights ( flights 10 and 13 made on December 9 and 11-12, respectively) enhancements of NOx ( NO + NO2) up to 1000 and 1600 parts per trillion by volume (pptv, 10-s data) were observed at altitudes between 11.5 and 14 km. The Geostationary Meteorological Satellite (GMS) cloud ( brightness temperature) data and ground-based lightning measurements by the Global Positioning and Tracking System (GPATS) indicate that there were intensive lightning events over the coast of the Gulf of Carpentaria, which took place upstream from our measurement area 10 to 14 h prior to the measurements. For these two flights, air in which NOx exceeded 100 pptv extended over 620 x 140 and 400 x 170 km(2) ( wind direction x perpendicular direction), respectively, suggesting a significant impact of lightning NO production on NOx levels in the tropics. We estimate the amount of NOx observed between 11.5 and 14 km produced by the thunderstorms to be 3.3 and 1.8 x 10(29) NO molecules for flights 10 and 13, respectively. By using the GPATS lightning flash count data, column NO production rates are estimated to be 1.9-4.4 and 21-49 x 10(25) NO molecules per single flash for these two flight data sets. In these estimations, it is assumed that the column NO production between 0 and 16 km is greater than the observed values between 11.5 and 14 km by a factor of 3.2, which is derived using results reported by Pickering et al. (1998). There are however large uncertainties in the GPATS lightning data in this study and care must be made when the production rates are referred. Uncertainties in these estimates are discussed. The impact on the ozone production rate is also described. C1 Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo 113, Japan. Univ Tokyo, Adv Sci & Technol Res Ctr, Tokyo 113, Japan. Kyoto Univ, Grad Sch Sci, Dept Earth & Planetary Sci, Ibaraki, Japan. Japan Aerosp Explorat, Earth Observ Res & Applicat Ctr, Tokyo, Japan. Univ Calif Irvine, Irvine, CA USA. Natl Inst Environm Studies, Ibaraki, Japan. Natl Inst Water & Atmospher Res Ltd, Lauder, New Zealand. NASA Langley Res Ctr, Hampton, VA USA. Osaka Univ, Grad Sch Engn, Dept Commun Engn, Osaka, Japan. RP Koike, M (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo 113, Japan. EM koike@eps.s.u-tokyo.ac.jp; kondo@atmos.rcast.u-tokyo.ac.jp; kita@env.sci.ibaraki.ac.jp; takegawa@atmos.rcast.u-tokyo.ac.jp; nishi@kugi.kyoto-u.ac.jp; kawakami.shuji@jaxa.jp; skudoh@eps.s.u-tokyo.ac.jp; drblake@uci.edu; tshirai@nies.go.jp; b.liley@niwa.co.nz; malcolm.k.ko@nasa.gov; yuzom@atmos.rcast.u-tokyo.ac.jp; zen@comm.eng.osaka-u.ac.jp; ogawa.toshihiro@jaxa.jp RI Koike, Makoto/F-4366-2011; Kondo, Yutaka/D-1459-2012; Miyazaki, Yuzo/C-6920-2010; Ko, Malcolm/D-5898-2015; OI Liley, Ben/0000-0002-8844-7928 NR 58 TC 9 Z9 10 U1 3 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 19 PY 2007 VL 112 IS D18 AR D18304 DI 10.1029/2006JD008193 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 213RN UT WOS:000249684900002 ER PT J AU Bleacher, JE Greeley, R Williams, DA Cave, SR Neukum, G AF Bleacher, Jacob E. Greeley, Ronald Williams, David A. Cave, Shelby R. Neukum, Gerhard TI Trends in effusive style at the Tharsis Montes, Mars, and implications for the development of the Tharsis province SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID THERMAL EMISSION SPECTROMETER; ORBITER LASER ALTIMETER; KILAUEA VOLCANO; ALBA-PATERA; LAVA FLOWS; ARSIA MONS; DIKE EMPLACEMENT; MARTIAN VOLCANOS; CERBERUS FOSSAE; HECATES-THOLUS AB We mapped lava flows on the Tharsis Montes (Arsia Mons, Pavonis Mons, and Ascraeus Mons) using High Resolution Stereo Camera images that centrally transect each shield from north to south, covering similar to 20% of each shield's surface. These data were co-registered to Mars Orbiter Laser Altimeter, Thermal Emission Imaging System, and Mars Orbiter Camera data, enabling lava flow structures and vents to be consistently differentiated across each volcano. Lava flow and vent abundances and relationships are used to provide new insight into the late Amazonian eruptive history of the Tharsis Montes. The volcanoes are divided into their main flanks, rift aprons, and small-vent fields. Where present on the main flanks, channel-fed flows always embay tube-fed flows, indicating a change from long-lived, stable tube-forming eruption conditions to shorter-lived, less stable channel-forming eruption conditions. Superposition relationships suggest that main flank and rift apron development were likely separated by an eruptive hiatus. The rift aprons, as compared to the main flanks, show higher abundances of tube-and channel-fed flows, and embayment of tube-fed flows by channel-fed flows is less consistent. Several trends from the Arsia Mons, to Ascraeus Mons, southwest rift aprons and small-vent fields were identified, including increased tube abundance, median slope, and number of satellitic eruptive vents and a decrease in channel-to tube-fed flow ratios, apron volumes, and maximum apron elevations. These trends suggest that the most recent volcanic activity at the Tharsis Montes might have originated from a single, shared magma source, possibly marking a change in magma production style from main flank construction. C1 NASA, Goddard Space Flight Ctr, Planetary & Geodynam Lab, Greenbelt, MD 20771 USA. Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. Freie Univ, Inst Geol Sci, D-12249 Berlin, Germany. RP Bleacher, JE (reprint author), NASA, Goddard Space Flight Ctr, Planetary & Geodynam Lab, Code 698,Bldg 33,Room G310, Greenbelt, MD 20771 USA. EM jake@puuoo.gsfc.nasa.gov RI Bleacher, Jacob/D-1051-2012 OI Bleacher, Jacob/0000-0002-8499-4828 NR 119 TC 45 Z9 45 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 19 PY 2007 VL 112 IS E9 AR E09005 DI 10.1029/2006JE002873 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 213SY UT WOS:000249688600001 ER PT J AU Wu, ZH Huang, NE Long, SR Peng, CK AF Wu, Zhaohua Huang, Norden E. Long, Steven R. Peng, Chung-Kang TI On the trend, detrending, and variability of nonlinear and nonstationary time series SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Empirical Mode Decomposition; global warming; intrinsic mode function; intrinsic trend; trend time scale ID EMPIRICAL MODE DECOMPOSITION; HILBERT SPECTRUM AB Determining trend and implementing detrending operations are important steps in data analysis. Yet there is no precise definition of "trend" nor any logical algorithm for extracting it. As a result, various ad hoc extrinsic methods have been used to determine trend and to facilitate a detrending operation. In this article, a simple and logical definition of trend is given for any nonlinear and nonstationary time series as an intrinsically determined monotonic function within a certain temporal span (most often that of the data span), or a function in which there can be at most one extremum within that temporal span. Being intrinsic, the method to derive the trend has to be adaptive. This definition of trend also presumes the existence of a natural time scale. All these requirements suggest the Empirical Mode Decomposition (EMD) method as the logical choice of algorithm for extracting various trends from a data set. Once the trend is determined, the corresponding detrending operation can be implemented. With this definition of trend, the variability of the data on various time scales also can be derived naturally. Climate data are used to illustrate the determination of the intrinsic trend and natural variability. C1 Harvard Univ, Sch Med, Beth Israel Deaconess Med Ctr, Div Interdisciplinary Med & Biotechnol, Boston, MA 02215 USA. Ctr Ocean Land Atmosphere Studies, Beltsville, MD 20705 USA. Natl Cent Univ, Res Ctr Adapt Data Anal, Chungli 32054, Taiwan. NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Ocean Sci Branch, Wallops Isl, VA 23337 USA. RP Wu, ZH (reprint author), Harvard Univ, Sch Med, Beth Israel Deaconess Med Ctr, Div Interdisciplinary Med & Biotechnol, Boston, MA 02215 USA. EM zhwu@cola.iges.org RI Peng, Chung-Kang/E-1489-2011; Long, Steven/D-7248-2012; Wu, Zhaohua/N-7102-2013; OI Peng, Chung-Kang/0000-0003-3666-9833; Wu, Zhaohua/0000-0003-1660-0724 FU NCRR NIH HHS [P41 RR013622, P41-RR13622] NR 16 TC 273 Z9 307 U1 16 U2 80 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 SEP 18 PY 2007 VL 104 IS 38 BP 14889 EP 14894 DI 10.1073/pnas.0701020104 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 214DB UT WOS:000249715100005 PM 17846430 ER PT J AU Give'on, A Belikov, R Shaklan, S Kasdin, J AF Give'on, Amir Belikov, Ruslan Shaklan, Stuart Kasdin, Jeremy TI Closed loop, DM diversity-based, wavefront correction algorithm for high contrast imaging systems SO OPTICS EXPRESS LA English DT Article AB High contrast imaging from space relies on coronagraphs to limit diffraction and a wavefront control systems to compensate for imperfections in both the telescope optics and the coronagraph. The extreme contrast required (up to 10(-10) for terrestrial planets) puts severe requirements on the wavefront control system, as the achievable contrast is limited by the quality of the wavefront. This paper presents a general closed loop correction algorithm for high contrast imaging coronagraphs by minimizing the energy in a predefined region in the image where terrestrial planets could be found. The estimation part of the algorithm reconstructs the complex field in the image plane using phase diversity caused by the deformable mirror. This method has been shown to achieve faster and better correction than classical speckle nulling. (c) 2007 Optical Society of America. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Princeton Univ, Princeton, NJ 08544 USA. RP Give'on, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM amir.giveon@jpl.nasa.gov NR 11 TC 45 Z9 45 U1 0 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD SEP 17 PY 2007 VL 15 IS 19 BP 12338 EP 12343 DI 10.1364/OE.15.012338 PG 6 WC Optics SC Optics GA 218HK UT WOS:000250006400065 PM 19547602 ER PT J AU Morales-Cruz, AL Fachini, ER Miranda, FA Cabrera, CR AF Morales-Cruz, Angel L. Fachini, Estevao R. Miranda, Felix A. Cabrera, Carlos R. TI Surface analysis monitoring of polyelectrolyte deposition on Ba0.5Sr0.5TiO3 thin films SO APPLIED SURFACE SCIENCE LA English DT Article DE BSTO; polyelectrolytes; self-assemblies; XPS; polystyrene sulfonate sodium; polyvinylsulfate potassium; polyallylamine hydrochloride ID ATOMIC-FORCE MICROSCOPY; ORDERED STRUCTURE; WATER; SPECTROSCOPY; MORPHOLOGY; POLYMERS; SYSTEM AB Thin films are currently gaining interest in many areas such as integrated optics, sensors, friction, reducing coatings, surface orientation layers, and general industrial applications. Recently, molecular self-assembling techniques have been applied for thin film deposition of electrically conducting polymers, conjugated polymers for light-emitting devices, nanoparticles, and noncentrosymmetric-ordered second order nonlinear optical (NOL) devices. Polyelectrolytes self-assemblies have been used to prepare thin films. The alternate immersion of a charged surface in polyannion and a polycation solution leads usually to the formation of films known as polyelectrolyte multilayers. These polyanion and polycation structures are not neutral. However, charge compensation appears on the surface. This constitutes the building driving force of the polyelectrolyte multilayer films. The present approach consists of two parts: (a) the chemisorption of 11-mercaptoundecylamine (MUA) to construct a self-assembled monolayer with the consequent protonation of the amine, and (b) the deposition of opposite charged polyelectrolytes in a sandwich fashion. The approach has the advantage that ionic attraction between opposite charges is the driving force for the multilayer buildup. For our purposes, the multilayer of polyelectrolytes depends on the quality of the surface needed for the application. In many cases, this approach will be used in a way that the roughness factor defects will be diminished. The polyelectrolytes selected for the study were: polystyrene sulfonate sodium salt (PSS), poly vinylsulfate potassium salt (PVS), and polyallylamine hydrochloride (PAH), as shown in Fig. 1. The deposition of polyelectrolytes was carried out by a dipping procedure with the corresponding polyelectrolyte. Monitoring of the alternate deposition of polyelectrolyte bilayers was done by surface analysis techniques such as X-ray photoelectron spectroscopy (XPS), specular reflectance infrared (IR), and atomic force microscopy (AFM). The surface analysis results are presented through the adsorption steps of the polyelectrolytes layer by layer. (c) 2007 Published by Elsevier B.V. C1 Univ Puerto Rico, Ctr Nanoscale Mat, Dept Chem, San Juan, PR 00931 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Cabrera, CR (reprint author), Univ Puerto Rico, Ctr Nanoscale Mat, Dept Chem, Rio Piedras Campus, San Juan, PR 00931 USA. EM ccabrera@upnp.edu OI Cabrera, Carlos/0000-0002-3342-8666 NR 28 TC 4 Z9 4 U1 0 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-4332 J9 APPL SURF SCI JI Appl. Surf. Sci. PD SEP 15 PY 2007 VL 253 IS 22 BP 8846 EP 8857 DI 10.1016/j.apsusc.2007.03.005 PG 12 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 210VQ UT WOS:000249484100007 ER PT J AU Kohout, T Kosterov, A Jackson, M Pesonen, LJ Kletetschka, G Lehtinen, M AF Kohout, T. Kosterov, A. Jackson, M. Pesonen, L. J. Kletetschka, G. Lehtinen, M. TI Low-temperature magnetic properties of the Neuschwanstein EL6 meteorite SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Neuschwanstein meteorite; daubreelite; troilite; kamacite; magnetism; magnetomineralogy; magnetic properties ID FERRIMAGNETIC FECR2S4; SINGLE-CRYSTALS; IRON SULFIDE; SUSCEPTIBILITY; SPECTROSCOPY; MOSSBAUER; TROILITE; FALL AB The low-temperature magnetic properties of the Neuschwanstein EL6 meteorite as well as of the daubreelite (FeCr2S4), troilite (Fes), and FeNi mineral phases were investigated. Low-temperature magnetic behavior of the Neuschwanstein meteorite appears to be controlled mostly by FeNi. However, two magnetic features at similar to 70 K (T.) and 150 K (T-c), are due to a magnetic transition in and Curie temperature of ferrimagnetic daubreelite. The similar to 10 K variations in T-m and T-c among daubreelite in the Neuschwanstein meteorite, daubreelite from the Coahuila meteorite and synthetic daubreelite [Tsurkan, V, Baran, M., Szymczak, R., Szymczak, H., Tidecks, R., 2001 a. Spin-glass like states in the ferrimagnet FeCr2S4. Physica B, 296, 301-305.] might be due to slightly different Fe/Cr stoichiometric ratios, the presence of impurities, or crystalline lattice defects. In the antiferromagnetic troilite a magnetic transition at T-m similar to 60 K was identified. Its nature seems to be most likely due to a change in the orientation and attendant canting of the antiparallel spins. However, this feature was not identified in the Neuschwanstein meteorite measurements because of low concentration and weak magnetization of the troilite phase compared to those of FeNi and daubreelite. Daubreelite with its Tc similar to 160 K might be a significant magnetic mineral in cold environment. Low-temperature magnetic data of daubreelite, troilite and FeNi presented here are useful for the interpretation of the low-temperature magnetic measurements of various extraterrestrial materials and for the identification of the presence of these phases. (C) 2007 Elsevier B.V All rights reserved. C1 Univ Helsinki, Div Geophys, FIN-00014 Helsinki, Finland. Charles Univ Prague, Dept Appl Geophys, CR-11636 Prague 1, Czech Republic. Acad Sci Czech Republic, Inst Geol, Prague, Czech Republic. Univ Minnesota, Inst Rock Magnetism, Minneapolis, MN USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Univ Helsinki, Geol Museum, FIN-00014 Helsinki, Finland. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kohout, T (reprint author), Univ Helsinki, Div Geophys, FIN-00014 Helsinki, Finland. EM tomas.kohout@helsinki.fi RI Kletetschka, Gunther/C-9996-2011; Kohout, Tomas/C-1394-2008; Kosterov, Andrei/I-4915-2012; Jackson, Mike/G-1587-2013 OI Kletetschka, Gunther/0000-0002-0645-9037; Kohout, Tomas/0000-0003-4458-3650; Kosterov, Andrei/0000-0001-8892-9698; Jackson, Mike/0000-0003-4778-7157 NR 25 TC 11 Z9 11 U1 1 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD SEP 15 PY 2007 VL 261 IS 1-2 BP 143 EP 151 DI 10.1016/j.epsl.2007.06.022 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 218VE UT WOS:000250042500012 ER PT J AU Brandon, AD Graham, DW Waight, T Gautason, B AF Brandon, Alan D. Graham, David W. Waight, Tod Gautason, Bjarm TI Os-186 and Os-187 enrichments and high-He-3/He-4 sources in the Earth's mantle: Evidence from Icelandic picrites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Review ID RECYCLED OCEANIC LITHOSPHERE; HELIUM ISOTOPIC SYSTEMATICS; CONVERGENT PLATE MARGIN; RE-OS; SUBDUCTION ZONES; HIGH HE-3/HE-4; OS-186-OS-187 SYSTEMATICS; SIDEROPHILE ELEMENTS; HAWAIIAN PICRITES; IRON-METEORITES AB Picrites from the neovolcanic zones in Iceland display a range in (OS)-O-187/(OS)-O-188 from 0.1297 to 0.1381 (gamma(Os) = +2.1 to -8.7) and uniform (OS)-O-186/(OS)-O-188 of 0.1198375 +/- 32 (2 sigma). The value for (OS)-O-186/(OS)-O-188 is within uncertainty of the present-day value for the primitive upper mantle of 0.1198398 +/- 16. These Os isotope systematics are best explained by ancient recycled crust or melt enrichment in the mantle source region. If so, then the coupled enrichments displayed in (OS)-O-186/(OS)-O-188 and (OS)-O-187/(OS)-O-188 from lavas of other plume systems must result from an independent process, the most viable candidate at present remains core-mantle interaction. While some plumes with high He-3/He-4, such as Hawaii, appear to have been subjected to detectable addition of Os (and possibly He) from the outer core, others such as Iceland do not. A positive correlation between (OS)-O-187/(OS)-O-188 and He-3/He-4 from 9.6 to 19 Ra in Iceland picrites is best modeled as mixtures of I Ga or older ancient recycled crust mixed with primitive mantle or incompletely degassed depleted mantle isolated since 1-1.5 Ga, which preserves the high He-3/He-4 of the depleted mantle at the time. These mixtures create a hybrid source region that subsequently mixes with the present-day convecting MORB mantle during ascent and melting. This multistage mixing scenario requires convective isolation in the deep mantle for hundreds of million years or more to maintain these compositionally distinct hybrid sources. The He-3/He-4 of lavas derived from the Iceland plume changed over time, from a maximum of 50 Ra at 60 Ma, to approximately 25-27 Ra at present. The changes are coupled with distinct compositional gaps between the different aged lavas when He-3/He-4 is plotted versus various geochemical parameters such as Nd-143/Nd-144 and La/Sm. These relationships can be interpreted as an increase in the proportion of ancient recycled crust in the upwelling plume over this time period. The positive correlation between Os-187/Os-188 and He-3/He-4 demonstrates that the Iceland lava He isotopic compositions do not result from simple melt depletion histories and consequent removal of U and Th in their mantle sources. Instead their He isotopic compositions reflect mixtures of heterogeneous materials formed at different times with different U and Th concentrations. This hybridization is likely prevalent in all ocean island lavas derived from deep mantle sources. Published by Elsevier Ltd. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. Inst Geol, DK-1350 Copenhagen, Denmark. Univ Akureyri, Iceland Geosurvey, IS-602 Akureyri, Iceland. RP Brandon, AD (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KR, Houston, TX 77058 USA. EM alan.d.brandonl@jsc.nasa.gov RI Waight, Tod/A-8262-2010; Gautason, Bjarni/N-6946-2013; OI Waight, Tod/0000-0003-2601-1202; Gautason, Bjarni/0000-0001-5909-8880; Graham, David/0000-0002-7411-1905 NR 106 TC 51 Z9 51 U1 2 U2 19 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 SEP 15 PY 2007 VL 71 IS 18 BP 4570 EP 4591 DI 10.1016/j.gea.2007.07.015 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 220OJ UT WOS:000250165700011 ER PT J AU Mou, S Li, JV Chuang, SL AF Mou, Shin Li, Jian V. Chuang, Shun Lien TI Surface channel current in InAs/GaSb type-II superlattice photodiodes SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID PASSIVATION AB We observed experimental evidences of surface channel current on the sidewall of InAs/GaSb superlattice photodiodes. We investigated the surface channel current by measuring the current-voltage (I-V) characteristics of the diodes. The experimental data compare very well with our theoretical model before and after ammonium sulfide passivation. By using the passivation, we reduced the surface channel current by five times, which supports that the surface channel current is induced by surface carriers. We believe that the surface channel current results from the inversion layer of a p-type superlattice with surface Fermi levels pinned above the conduction-band minimum in InAs/GaSb superlattices. C1 Univ Illinois, Dept Elect & Comp Engn, Urbana, IL 61801 USA. RP Mou, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. EM s-chuang@uiuc.edu RI Li, Jian/B-1627-2016 NR 13 TC 10 Z9 10 U1 3 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 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD SEP 15 PY 2007 VL 102 IS 6 AR 066103 DI 10.1063/1.2783767 PG 3 WC Physics, Applied SC Physics GA 215CZ UT WOS:000249787200128 ER PT J AU Suh, JO Tu, KN Tamura, N AF Suh, J. O. Tu, K. N. Tamura, N. TI Preferred orientation relationship between Cu6Sn5 scallop-type grains and Cu substrate in reactions between molten Sn-based solders and Cu SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID X-RAY-DIFFRACTION; LEAD-FREE SOLDERS; INTERMETALLIC COMPOUNDS; COMPOUND; JOINTS; NI; AG AB A strong crystallographic orientation relationship between the Cu6Sn5 scallop-type grains and their Cu substrate has been found by synchrotron micro-x-ray diffraction study. Even though the crystal structures of Cu6Sn5 (monoclinic) and Cu (face-centered-cubic) are very different, angular distributions of crystallographic directions between Cu6Sn5 and Cu revealed a strong orientation relationship. Both SnPb solder and pure Sn showed the same result, indicating that this is general behavior between Sn-based solders and Cu. The strong orientation relation suggests that Cu6Sn5 forms prior to Cu3Sn in the wetting reactions. A total of six different orientation relationships were found. In all the cases, the [(1) over bar 101] direction of Cu6Sn5 preferred to be parallel to the [110] direction of Cu with a misfit of 0.24%. Due to pseudohexagonal structure of the Cu6Sn5, the six relationships can be categorized into two groups. From the orientation distribution, one group was found to be less rigid then the other group. (C) 2007 American Institute of Physics. C1 Univ Calif Los Angeles, Dept Mat Sci & Engn, Los Angeles, CA 90095 USA. Ernest Orlando Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Suh, JO (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA. EM Jong-ook.Suh@jpl.nasa.gov NR 18 TC 45 Z9 46 U1 4 U2 30 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 J9 J APPL PHYS JI J. Appl. Phys. PD SEP 15 PY 2007 VL 102 IS 6 AR 063511 DI 10.1063/1.2776002 PG 7 WC Physics, Applied SC Physics GA 215CZ UT WOS:000249787200032 ER PT J AU Bulow, RC Johnson, CL Bills, BG Shearer, PM AF Bulow, R. C. Johnson, C. L. Bills, B. G. Shearer, P. M. TI Temporal and spatial properties of some deep moonquake clusters SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LUNAR SEISMIC DATA; TIDAL STRESSES; MOON; TECTONICS; MODEL AB Using the event search method of Bulow et al. ( 2005), we have found 503 new deep moonquakes among the eight largest ( in terms of total number) nearside source regions, increasing the number of identified events for each cluster an average of 36% over the existing catalog. These new events provide an improved deep event catalog, with which we explore some temporal and spatial aspects of deep moonquakes. First, we examine the spectra of moonquake occurrence times at each deep source region, and observe known tidal periodicities, notably those at similar to 27 days and 206 days. Application of spectral methods for the analyses of point processes ( discrete events) allows us to resolve closely spaced tidal periods not previously seen in moonquake data. Second, we pick seismic phase arrival times from optimized stacks of events from each source region. We use these picks, along with published velocity models, to relocate the nine source regions. Source regions A1 and A18 are the best located, with 95% confidence bounds of less than +/- 5 degrees in latitude and longitude, and consistent with estimates from different studies. The locations of source regions A8 and A9 are poorly constrained, with uncertainties in latitude of up to +/- 28 degrees resulting from the absence of clear phase arrivals at station 15. Large trade-offs exist between relocation estimates and choice of velocity model, and the lack of reliable seismic phase arrivals severely affects location error. C1 Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA USA. Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC, Canada. NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Bulow, RC (reprint author), Inst Phys Globe, St Maur De Fosses, France. EM bulow@ipgp.jussieu.fr RI Bills, Bruce/C-1156-2008; Shearer, Peter/K-5247-2012 OI Shearer, Peter/0000-0002-2992-7630 NR 21 TC 13 Z9 13 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 15 PY 2007 VL 112 IS E9 AR E09003 DI 10.1029/2006JE002847 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 211JK UT WOS:000249519900001 ER PT J AU Fu, DJ Boone, CD Bernath, PF Walker, KA Nassar, R Manney, GL McLeod, SD AF Fu, Dejian Boone, Chris D. Bernath, Peter F. Walker, Kaley A. Nassar, Ray Manney, Gloria L. McLeod, Sean D. TI Global phosgene observations from the atmospheric chemistry experiment (ACE) mission SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID STRATOSPHERIC CHLORINE; HALOCARBONS; TROPOSPHERE; PACIFIC; AIR AB The first study of the global distribution of atmospheric phosgene (COCl2) has been performed using solar occultation measurements from the Atmospheric Chemistry Experiment ( ACE) satellite mission. A total of 5614 measured profiles spanning the period February 2004 through May 2006 were used in the study. The phosgene concentrations display a zonally symmetric pattern with the maximum concentration located approximately over the equator at about 25 km in altitude and the concentration decreases towards the poles. A layer of enhanced concentration of phosgene spans the lower stratosphere over all latitudes, with volume mixing ratios of 20-60 pptv. The ACE observations show lower phosgene concentrations in the stratosphere than were obtained from previous observations in the 1980s and 1990s. This has been attributed to a significant decrease in its source species, particularly two major sources CH3CCl3 and CCl4, since the introduction of restrictions required by the Montreal Protocol and its amendments. C1 Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. Univ Toronto, Dept Phys, Toronto, ON, Canada. CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. New Mexico Highlands Univ, Dept Nat Sci, Las Vegas, NM USA. RP Fu, DJ (reprint author), Univ Waterloo, Dept Chem, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada. EM dfu@acebox.uwaterloo.ca RI Bernath, Peter/B-6567-2012; OI Bernath, Peter/0000-0002-1255-396X; Nassar, Ray/0000-0001-6282-1611 NR 27 TC 11 Z9 11 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 14 PY 2007 VL 34 IS 17 AR L17815 DI 10.1029/2007GL029942 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 211IT UT WOS:000249518200001 ER PT J AU Santanello, JA Peters-Lidard, CD Garcia, ME Mocko, DM Tischler, MA Moran, MS Thoma, DP AF Santanello, Joseph A., Jr. Peters-Lidard, Christa D. Garcia, Matthew E. Mocko, David M. Tischler, Michael A. Moran, M. Susan Thoma, D. P. TI Using remotely-sensed estimates of soil moisture to infer soil texture and hydraulic properties across a semi-arid watershed SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE parameter estimation; soil moisture; active microwave; passive microwave; PBMR; land surface modeling; model calibration; soil hydraulic; properties; temporal sampling; watershed modeling; soil type; pedotransfer functions ID LAND-SURFACE MODEL; BOUNDARY-LAYER; PEDOTRANSFER FUNCTIONS; DATA ASSIMILATION; ETA-MODEL; CONDUCTIVITY; PARAMETERS; SIMULATION; ENERGY; FLOW AB Near-surface soil moisture is a critical component of land surface energy and water balance studies encompassing a wide range of disciplines. However, the processes of infiltration, runoff, and evapotranspiration in the vadose zone of the soil are not easy to quantify or predict because of the difficulty in accurately representing soil texture and hydraulic properties in land surface models. This study approaches the problem of parameterizing soil properties from a unique perspective based on components originally developed for operational estimation of soil moisture for mobility assessments. Estimates of near-surface soil moisture derived from passive (L-band) microwave remote sensing were acquired on six dates during the Monsoon '90 experiment in southeastern Arizona, and used to calibrate hydraulic properties in an offline land surface model and infer information on the soil conditions of the region. Specifically, a robust parameter estimation tool (PEST) was used to calibrate the Noah land surface model and run at very high spatial resolution across the Walnut Gulch Experimental Watershed. Errors in simulated versus observed soil moisture were minimized by adjusting the soil texture, which in turn controls the hydraulic properties through the use of pedotransfer functions. By estimating within a continuous range of widely applicable soil properties such as sand, silt, and clay percentages rather than applying rigid soil texture classes, lookup tables, or large parameter sets as in previous studies, the physical accuracy and consistency of the resulting soils could then be assessed. In addition, the sensitivity of this calibration method to the number and timing of microwave retrievals is determined in relation to the temporal patterns in precipitation and soil drying. The resultant soil properties were applied to an extended time period demonstrating the improvement in simulated soil moisture over that using default or county-level soil parameters. The methodology is also applied to an independent case at Walnut Gulch using a new soil moisture product from active (C-band) radar imagery with much lower spatial and temporal resolution. Overall, results demonstrate the potential to gain physically meaningful soil information using simple parameter estimation with few but appropriately timed remote sensing retrievals. (c) 2007 Elsevier Inc. All rights reserved. C1 UMCP, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Sci Applicat Int Corp, Mclean, VA 22102 USA. USA, Ctr Res Dev & Engn, TEC, Alexandria, VA USA. USDA ARS, SW Watershed Res Ctr, Tucson, AZ USA. UMBC, Goddard Earth Sci & Technol Ctr, Baltimore, MD USA. RP Santanello, JA (reprint author), UMCP, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. EM sntnello@hsb.gsfc.nasa.gov RI Santanello, Joseph/D-4438-2012; Garcia, Matthew/K-9286-2013; Peters-Lidard, Christa/E-1429-2012 OI Santanello, Joseph/0000-0002-0807-6590; Garcia, Matthew/0000-0002-9637-4204; Peters-Lidard, Christa/0000-0003-1255-2876 NR 69 TC 71 Z9 74 U1 2 U2 30 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 SEP 14 PY 2007 VL 110 IS 1 BP 79 EP 97 DI 10.1016/j.rse.2007.02.007 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 198PJ UT WOS:000248639700006 ER PT J AU Nelson, RF Hyde, P Johnson, P Emessiene, B Imhoff, ML Campbell, R Edwards, W AF Nelson, Ross F. Hyde, Peter Johnson, Patrick Emessiene, Bomono Imhoff, Marc L. Campbell, Robert Edwards, Wilson TI Investigating RaDAR-LiDAR synergy in a North Carolina pine forest SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE VHFRaDAR; profiling LiDAR; biomass; RaDAR-LiDAR synergy ID II VHFSAR DATA; SMALL-FOOTPRINT LIDAR; AIRBORNE LASER DATA; STEM VOLUME; STAND CHARACTERISTICS; AERIAL-PHOTOGRAPHY; VEGETATION BIOMASS; CONIFEROUS FOREST; BOREAL FORESTS; SCANNER DATA AB A low frequency (80-120 MHz) VHF RaDAR, BioSAR, specifically designed for forest biomass estimation and a profiling LiDAR, PALS, were flown over loblolly pine plantations in the southeastern United States. LiDAR-only, RaDAR-only, and joint LiDAR-RaDAR linear models were developed to determine if returns from two sensors could be used to estimate pine biomass more accurately and precisely than returns from either sensor alone. The best five-variable RaDAR model explained 81.8% (R (2)) of the stem green biomass variability, with a regression RMSE of 57.5 t/ha. The best one-variable LiDAR model explained 93.3% of the biomass variation (RMSE=33.9 t/ha). Combining the RaDAR normalized volumetric returns with the profiling LiDAR ranging measurements did little to improve the best LiDAR-only model. The best LiDAR-RaDAR model explained 93.8% of the biomass variation (RSME=32.7 t/ha). Cross-validation and training/test validation procedures demonstrated (1) that all models are unbiased and (2) the increased precision of the LiDAR-only and LiDAR-RaDAR models. The results of this investigation and a companion study indicate that there is little to be gained combining VHF-RaDAR volumetric returns and profiling LiDAR ranging measurements in pine forests; a LiDAR ranging system is sufficient for accurate, precise biomass estimation. 2007 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Zimmerman Associates Inc, Vienna, VA 22031 USA. Weyerhaeuser Inc, New Bern, NC 28563 USA. RP Nelson, RF (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 614-4, Greenbelt, MD 20771 USA. EM Ross.F.Nelson@nasa.gov RI Nelson, Ross/H-8266-2014 NR 50 TC 49 Z9 49 U1 3 U2 11 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 SEP 14 PY 2007 VL 110 IS 1 BP 98 EP 108 DI 10.1016/j.rse.2007.02.006 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 198PJ UT WOS:000248639700007 ER PT J AU Yang, FH Ichii, K White, MA Hashimoto, H Michaelis, AR Votava, P Zhu, AX Huete, A Running, SW Nemani, RR AF Yang, Feihua Ichii, Kazuhito White, Michael A. Hashimoto, Hirofumi Michaelis, Andrew R. Votava, Petr Zhu, A-Xing Huete, Alfredo Running, Steven W. Nemani, Ramakrishna R. TI Developing a continental-scale measure of gross primary production by combining MODIS and AmeriFlux data through Support Vector Machine approach SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE gross primary production; AmeriFlux; support vector machines; light use efficiency; moderate resolution Imaging spectroradiometer (MODIS) ID NET PRIMARY PRODUCTION; LAND-SURFACE TEMPERATURE; DECIDUOUS FOREST; CARBON-DIOXIDE; VEGETATION INDEXES; TERRESTRIAL GROSS; USE EFFICIENCY; LEAF-AREA; FLUX; VALIDATION AB Remote sensing is a potentially powerful technology with which to extrapolate eddy covariance-based gross primary production (GPP) to continental scales. In support of this concept, we used meteorological and flux data from the AmeriFlux network and Support Vector Machine (SVM), an inductive machine learning technique, to develop and apply a predictive GPP model for the conterminous U.S. In the following four-step process, we first trained the SVM to predict flux-based GPP from 33 AmeriFlux sites between 2000 and 2003 using three remotely-sensed variables (land surface temperature, enhanced vegetation index (EVI), and land cover) and one ground-measured variable (incident shortwave radiation). Second, we evaluated model performance by predicting GPP for 24 available AmeriFlux sites in 2004. In this independent evaluation, the SVM predicted GPP with a root mean squared error (RMSE) of 1.87 gC/m(2)/day and an R-2 of 0.71. Based on annual total GPP at 15 AmeriFlux sites for which the number of 8-day averages in 2004 was no less than 67%(30 out of a possible 45), annual SVM GPP prediction error was 32.1% for non-forest ecosystems and 22.2% for forest ecosystems, while the standard Moderate Resolution Imaging Spectroradiometer GPP product (MOD17) had an error of 50.3% for non-forest ecosystems and 21.5% for forest ecosystems, suggesting that the regionally tuned SVM performed better than the standard global MOD 17 GPP for non-forest ecosystems but had similar performance for forest ecosystems. The most important explanatory factor for GPP prediction was EVI, removal of which increased GPP RMSE by 0.85 gC/m2/day in a cross-validation experiment. Third, using the SVM driven by remote sensing data including incident shortwave radiation, we predicted 2004 conterminous U.S. GPP and found that results were consistent with expected spatial and temporal patterns. Finally, as an illustration of SVM GPP for ecological applications, we estimated maximum light use efficiency (e(max)), one of the most important factors for standard light use efficiency models, for the conterminous U.S. by integrating the 2004 SVM GPP with the MOD17 GPP algorithm. We found that emax varied from similar to 0.86 gC/MJ in grasslands to similar to 1.56 gC/MJ in deciduous forests, while MOD17 emax was 0.68 gC/MJ for grasslands and 1.16 gC/MJ for deciduous forests, suggesting that refinements of MOD17 emax may be beneficial. 2007 Elsevier Inc. All rights reserved. C1 Univ Wisconsin, Dept Geog, Madison, WI 53706 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. San Jose State Univ, San Jose, CA 95192 USA. Utah State Univ, Logan, UT 84322 USA. Calif State Univ, Monterey, CA USA. Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, State Key Lab Resources & Environm Informat Syst, Beijing 100864, Peoples R China. Univ Arizona, Tucson, AZ USA. Univ Montana, Missoula, MT 59812 USA. RP Yang, FH (reprint author), Univ Wisconsin, Dept Geog, 426 Sci Hall,550 N Pk St, Madison, WI 53706 USA. EM feihuayang@wisc.edu RI Ichii, Kazuhito/D-2392-2010; Huete, Alfredo/C-1294-2008; OI Ichii, Kazuhito/0000-0002-8696-8084; Huete, Alfredo/0000-0003-2809-2376; White, Michael/0000-0002-0238-8913 NR 54 TC 88 Z9 98 U1 6 U2 26 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 SEP 14 PY 2007 VL 110 IS 1 BP 109 EP 122 DI 10.1016/j.rse.2007.02.016 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 198PJ UT WOS:000248639700008 ER PT J AU Thomas, GW Peate, IU Nakamoto, J Pudenz, E Glasgow, J Bretthauer, J Cabrol, N Wettergreen, D Grin, E Coppin, P Dohm, JM Piatek, JL Warren-Rhodes, K Hock, AN Weinstein, S Fisher, G Diaz, GC Cockell, CS Marinangeli, L Minkley, N Moersch, J Ori, GG Smith, T Stubb, K Wagner, M Waggoner, AS AF Thomas, G. W. Peate, I. Ukstins Nakamoto, J. Pudenz, E. Glasgow, J. Bretthauer, J. Cabrol, N. Wettergreen, D. Grin, E. Coppin, P. Dohm, J. M. Piatek, J. L. Warren-Rhodes, K. Hock, A. N. Weinstein, S. Fisher, G. Diaz, G. Chong Cockell, C. S. Marinangeli, L. Minkley, N. Moersch, J. Ori, G. G. Smith, T. Stubb, K. Wagner, M. Waggoner, A. S. TI Comparing different methods for assessing ground truth of rover data analysis for the 2005 season of the Life in the Atacama Project SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID THEMATIC MAPPER DATA; NORTHWEST-TERRITORIES; FIELD EXPERIMENT; MARS; MISSIONS; HABITAT; SCIENCE; DESERT AB The scientific success of a remote exploration rover mission depends on the right combination of technology, teamwork and scientific insight. In order to quantitatively evaluate the success of a rover field trial, it is necessary to assess the accuracy of scientific interpretations made during the field test. This work compares three structured approaches to assessing the ground truth of scientific findings from a science team conducting a remote investigation of a locale using an autonomous rover. For the first approach, independent assessment, the daily science summaries were analyzed and reduced to a series of 1082 factual statements, which were treated as hypotheses. An independent scientist traveled to the field area to assess these hypotheses. For the second approach, guided self-study, the mission scientists themselves traveled to the field area and evaluated their own scientific interpretations. The third approach, discrepancy investigation, searched for the root causes of differences between the scientific interpretations made in the control room and those made in the field. The independent investigation provided sensitive, quantitative data, but suffered from the lack of context and continuity developed in the mission control room. The guided evaluation benefited from the context of the mission, but lacked clarity and consistency. The discrepancy investigation provided insight into the root causes behind the discrepancies, but was expensive and time consuming. The independent investigation method yielded particularly compelling results, but each method offers advantages and a comprehensive rover field trial assessment should include a combination of all three. C1 Univ Iowa, Dept Mech & Ind Engn, Iowa City, IA 52242 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA USA. Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. Carnegie Mellon Univ, Mol Biosensor & Imaging Ctr, Pittsburgh, PA 15213 USA. Univ Catholica Norte, Antofagasta, Chile. British Antarctic Survey, Cambridge CB3 0ET, England. IRSPS, I-65127 Pescara, Italy. RP Thomas, GW (reprint author), Univ Iowa, Dept Mech & Ind Engn, Iowa City, IA 52242 USA. RI Moersch, Jeffrey/F-7189-2010; Dohm, James/A-3831-2014; OI ORI, Gian Gabriele/0000-0002-6460-1476 NR 38 TC 1 Z9 1 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD SEP 13 PY 2007 VL 112 IS G4 AR G04S09 DI 10.1029/2006JG000318 PG 12 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 211JC UT WOS:000249519100002 ER PT J AU Warren-Rhodes, KA Dungan, JL Piatek, J Stubbs, K Gomez-Silva, B Chen, Y Mckay, CP AF Warren-Rhodes, Kimberley A. Dungan, Jennifer L. Piatek, Jennifer Stubbs, Kristin Gomez-Silva, Benito Chen, Yong Mckay, Christopher P. TI Ecology and spatial pattern of cyanobacterial community island patches in the Atacama Desert, Chile SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID CRYPTOENDOLITHIC MICROBIAL ENVIRONMENT; ROSS DESERT; SOIL; LANDSCAPES; ANTARCTICA; SCALES; CRUSTS; ALGAE; HOT; TEMPERATURE AB Plant landscape ecology studies have been carried out for decades and are fundamental to biological research. In contrast, few corollary spatial landscape studies exist for microorganisms, particularly in extreme environments. To address this gap, we mapped the abundance and spatial distribution of photoautotrophs colonizing translucent rocks in several sites in the Atacama Desert, including the hyperarid core. Cyanobacterial communities at all sites are predominantly (>= 75%) 'perilithic' (confined to the periphery of rocks) and occur in non-random spatial patterns ("island patches'') at multiple scales. Cyanobacterial patches typically contain 1-5 colonized rocks but in some cases support much higher numbers. A high resolution mapping of a single 18-m(2) rock cluster at the Aguas Calientes study site (25 degrees S, 69 degrees W) revealed colonization of 5.2% (49 of 948 quartz rocks) and showed colonized rocks to be much larger (similar to 2X) than the available mean rock size. Ripley's K and point pattern analyses show that quartz rocks are not "selected'' or occupied by cyanobacteria randomly, but that non-random processes distinct from those creating the background rock pattern must be invoked to explain microbial patchiness in the Atacama Desert. These processes include physical controls (rock size/orientation, microtopography) that reflect resource (water) limitations, and biological dispersal via rainfall, fog and wind. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. Univ Antofagasta, Dept Biomed, Antofagasta, Chile. Univ Antofagasta, Inst Desierto, Antofagasta, Chile. Univ Iowa, Dept Mech & Ind Engn, Iowa City, IA USA. RP Warren-Rhodes, KA (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA. RI Dungan, Jennifer/G-9921-2016 OI Dungan, Jennifer/0000-0002-4863-1616 NR 83 TC 13 Z9 14 U1 1 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD SEP 13 PY 2007 VL 112 IS G4 AR G04S15 DI 10.1029/2006JG000305 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 211JC UT WOS:000249519100001 ER PT J AU Fortney, J AF Fortney, Jonathan TI Extrasolar planets - The one that got away SO NATURE LA English DT Editorial Material ID SYSTEM C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fortney, J (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM jfortney@arc.nasa.gov OI Fortney, Jonathan/0000-0002-9843-4354 NR 10 TC 1 Z9 1 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD SEP 13 PY 2007 VL 449 IS 7159 BP 147 EP 148 DI 10.1038/449147a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 209NF UT WOS:000249394500025 PM 17851500 ER PT J AU Schorghofer, N AF Schorghofer, Norbert TI Dynamics of ice ages on Mars SO NATURE LA English DT Article ID GROUND ICE; ASTRONOMICAL THEORY; HIGH OBLIQUITY; NEAR-SURFACE; DEPOSITS; PRECIPITATION; INSOLATION; LATITUDES; STABILITY; HYDROGEN AB Unlike Earth, where astronomical climate forcing is comparatively small, Mars experiences dramatic changes in incident sunlight that are capable of redistributing ice on a global scale(1-6). The geographic extent of the subsurface ice found poleward of approximately +/-60 degrees latitude on both hemispheres of Mars(7-9) coincides with the areas where ice is stable(7,10,11). However, the tilt of Mars' rotation axis (obliquity) changed considerably in the past several million years. Earlier work(3,12) has shown that regions of ice stability, which are defined by temperature and atmospheric humidity, differed in the recent past from today's, and subsurface ice is expected to retreat quickly when unstable(11-13). Here I explain how the subsurface ice sheets could have evolved to the state in which we see them today. Simulations of the retreat and growth of ground ice as a result of sublimation loss and recharge reveal forty major ice ages over the past five million years. Today, this gives rise to pore ice at mid-latitudes and a three-layered depth distribution in the high latitudes of, from top to bottom, a dry layer, pore ice, and a massive ice sheet. Combined, these layers provide enough ice to be compatible with existing neutron and gamma-ray measurements(7-9). C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. RP Schorghofer, N (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM norbert@hawaii.edu RI Schorghofer, Norbert/A-1194-2007 NR 25 TC 58 Z9 59 U1 0 U2 10 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD SEP 13 PY 2007 VL 449 IS 7159 BP 192 EP U2 DI 10.1038/nature06082 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 209NF UT WOS:000249394500043 PM 17851518 ER PT J AU Weisz, E Li, J Menzel, WP Heidinger, AK Kahn, BH Liu, CY AF Weisz, Elisabeth Li, Jun Menzel, W. Paul Heidinger, Andrew K. Kahn, Brian H. Liu, Chian-Yi TI Comparison of AIRS, MODIS, CloudSat and CALIPSO cloud top height retrievals SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VARIATIONAL RETRIEVAL; PARAMETERS AB Knowledge of cloud properties like cloud top height (CTH) is essential to understand their impact on the earth's radiation budget and on climate change. High spectral resolution measurements from the Atmospheric Infrared Sounder (AIRS) are well suited to reveal valuable information about cloud altitude. The CTH retrievals derived from AIRS single field-of-view(FOV) radiance measurements are compared with the operational MODIS ( Moderate Resolution Imaging Spectroradiometer) cloud product, and Level 2 products obtained from radar and lidar instruments onboard the EOS (Earth Observing System) CloudSat and the CALIPSO (Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation) satellites. Two cases containing a variety of cloud conditions have been studied, and the strengths/shortcomings of CTH products from infrared (IR) sounder radiances are discussed. C1 Univ Wisconsin, CIMSS, Madison, WI 53706 USA. NOAA NESDIS Ctr Satellite Applicat & Res, Madison, WI 53706 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Weisz, E (reprint author), Univ Wisconsin, CIMSS, 1225 W Dayton St, Madison, WI 53706 USA. RI Menzel, W. Paul/B-8306-2011; Heidinger, Andrew/F-5591-2010; Liu, Chian-Yi/B-1898-2015; Li, Jun/H-3579-2015 OI Menzel, W. Paul/0000-0001-5690-1201; Heidinger, Andrew/0000-0001-7631-109X; Liu, Chian-Yi/0000-0003-1725-4405; Li, Jun/0000-0001-5504-9627 NR 17 TC 54 Z9 59 U1 2 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 11 PY 2007 VL 34 IS 17 AR L17811 DI 10.1029/2007GL030676 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 211IP UT WOS:000249517800001 ER PT J AU Ahmad, Z McClain, CR Herman, JR Franz, BA Kwiatkowska, EJ Robinson, WD Bucsela, EJ Tzortziou, M AF Ahmad, Ziauddin McClain, Charles R. Herman, Jay R. Franz, Bryan A. Kwiatkowska, Ewa J. Robinson, Wayne D. Bucsela, Eric J. Tzortziou, Maria TI Atmospheric correction for NO2 absorption in retrieving water-leaving reflectances from the SeaWiFS and MODIS measurements SO APPLIED OPTICS LA English DT Article ID NITROGEN-DIOXIDE; NM AB The absorption by atmospheric nitrogen dioxide (NO2) gas in the visible has been traditionally neglected in the retrieval of oceanic parameters from satellite measurements. Recent measurements of NO2 from spaceborne sensors show that over the Eastern United States the NO2 column amount often exceeds I Dobson Unit (similar to 2.69 X 10(16) molecules/cm(2)). Our radiative transfer sensitivity calculations show that under high NO2 conditions (similar to 1 x 10(16) molecules/cm(2)) the error in top-of-atmosphere (TOA) reflectance in the blue channels of the sea-viewing wide field-of-view sensor (SeaWiFS) and moderate-resolution imaging spectroradiometer (MODIS) sensors is approximately 1%. This translates into approximately 10% error in water-leaving radiance for clear waters and to higher values (>20%) in the coastal areas. We have developed an atmospheric-correction algorithm that allows an accurate retrieval of normalized water-leaving radiances (nLws) in the presence of NO2 in the atmosphere. The application of the algorithm to 52 MODIS scenes over the Chesapeake Bay area show a decrease in the frequency of negative nLw estimates in the 412 run band and an increase in the value of nLws in the same band. For the particular scene reported in this paper, the mean value of nLws in the 412 nm band increased by 17%, which is significant, because for the MODIS sensor the error in nLws attributable to the digitization error in the observed TOA reflectance over case 2 waters is similar to 2.5%. (c) 2007 Optical Society of America. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci & Data Syst Inc, Silver Spring, MD 20906 USA. Sci Applicat Int Corp, San Diego, CA 92121 USA. Univ Maryland, Baltimore, MD 21250 USA. Univ Maryland, College Pk, MD 20742 USA. RP Ahmad, Z (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ahmad@seawifs.gsfc.nasa.gov RI Franz, Bryan/D-6284-2012 OI Franz, Bryan/0000-0003-0293-2082 NR 17 TC 16 Z9 16 U1 0 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD SEP 10 PY 2007 VL 46 IS 26 BP 6504 EP 6512 DI 10.1364/AO.46.006504 PG 9 WC Optics SC Optics GA 220PP UT WOS:000250169000002 PM 17846643 ER PT J AU Jenkins, LP Hornschemeier, AE Mobasher, B Alexander, DM Bauer, FE AF Jenkins, L. P. Hornschemeier, A. E. Mobasher, B. Alexander, D. M. Bauer, F. E. TI Uncovering the near-IR dwarf galaxy population of the coma cluster with Spitzer IRAC SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (Coma); galaxies : luminosity function; mass function ID INFRARED LUMINOSITY FUNCTION; BACKGROUND EXPERIMENT SEARCH; ARRAY CAMERA IRAC; SPACE-TELESCOPE; GIANT GALAXIES; K-BAND; VIRGO CLUSTER; FAINT END; EVOLUTION; DYNAMICS AB We present the first results of a Spitzer IRAC ( Infrared Array Camera) wide-field survey of two regions of the Coma Cluster. The observations cover two fields; the first is a 0.733 deg(2) region in the core of the cluster ( Coma 1), the second a 0.555 deg(2) off-center region located similar to 57 ' (1.7 Mpc) southwest from the core ( Coma 3). The IRAC observations, although short 70-90 s exposures, are very sensitive; we detect similar to 29,200 sources at 3.6 mu m over the total similar to 1.3 deg(2) survey area. We construct 3.6 mu m galaxy luminosity functions (LFs) for each field using selection functions based on spectroscopic redshifts. At the bright end, the LFs are well modeled by a traditional Schechter function; < M*(3.6) mu m, alpha(1)> <-25.17, -1.18 > and <-24.69, -1.30 > for Coma 1 and Coma 3 respectively. However, at the faint end (M-3:6 mu m > -20.5) there is a steep increase in the LF slope in both fields indicative of large numbers of red dwarf galaxies. The reality of this population is examined using SDSS optical counterparts with optical color filtering ( g - r < 1: 3). The steep increase can be modeled with a power-law function, with slopes of alpha(2) = -2.18 (Coma 1) and alpha(2) = -2.60 (Coma 3), the difference likely indicating a change in environmental effects between the two fields. A qualitative comparison with optical (B- and R- band) LFs shows that we are likely to be observing a larger population of dwarf galaxies in the near-IR, which may be a low surface brightness (LSB) population that IRAC is particularly sensitive to, or a population too red to be detected in the existing optical surveys down to R similar to 20. C1 NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Durham, Durham DH1 3LE, England. Columbia Univ, New York, NY 10027 USA. RP Jenkins, LP (reprint author), NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. OI Jenkins, Leigh/0000-0001-9464-0719; Alexander, David/0000-0002-5896-6313 NR 77 TC 25 Z9 25 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2007 VL 666 IS 2 BP 846 EP 862 DI 10.1086/520035 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208FR UT WOS:000249305700019 ER PT J AU Calzetti, D Kennicutt, RC Engelbracht, CW Leitherer, C Draine, BT Kewley, L Moustakas, J Sosey, M Dale, DA Gordon, KD Helou, GX Hollenbach, DJ Armus, L Bendo, G Bot, C Buckalew, B Jarrett, T Li, A Meyer, M Murphy, EJ Prescott, M Regan, MW Rieke, GH Roussel, H Sheth, K Smith, JDT Thornley, MD Walter, F AF Calzetti, D. Kennicutt, R. C. Engelbracht, C. W. Leitherer, C. Draine, B. T. Kewley, L. Moustakas, J. Sosey, M. Dale, D. A. Gordon, K. D. Helou, G. X. Hollenbach, D. J. Armus, L. Bendo, G. Bot, C. Buckalew, B. Jarrett, T. Li, A. Meyer, M. Murphy, E. J. Prescott, M. Regan, M. W. Rieke, G. H. Roussel, H. Sheth, K. Smith, J. D. T. Thornley, M. D. Walter, F. TI The calibration of mid-infrared star formation rate indicators SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : interactions; galaxies : ISM; galaxies : starburst; ISM : structure ID POLYCYCLIC AROMATIC-HYDROCARBONS; SPECTRAL ENERGY-DISTRIBUTION; DEEP SUBMILLIMETER SURVEY; DWARF IRREGULAR GALAXIES; LARGE-MAGELLANIC-CLOUD; INFRARED ARRAY CAMERA; H-II REGIONS; FORMING GALAXIES; NEARBY GALAXIES; STARBURST GALAXIES AB With the goal of investigating the degree to which the MIR emission traces the SFR, we analyze Spitzer 8 and 24 mu m data of star-forming regions in a sample of 33 nearby galaxies with available HST NICMOS images in the Pa alpha (1.8756 mu m) emission line. The galaxies are drawn from the SINGS sample and cover a range of morphologies and a factor similar to 10 in oxygen abundance. Published data on local low-metallicity starburst galaxies and LIRGs are also included in the analysis. Both the stellar continuumYsubtracted 8 mu m emission and the 24 mu m emission correlate with the extinction-corrected Pa alpha line emission, although neither relationship is linear. Simple models of stellar populations and dust extinction and emission are able to reproduce the observed nonlinear trend of the 24 mu m emission versus number of ionizing photons, including the modest deficiency of 24 mu m emission in the low-metallicity regions, which results from a combination of decreasing dust opacity and dust temperature at low luminosities. Conversely, the trend of the 8 mu m emission as a function of the number of ionizing photons is not well reproduced by the same models. The 8 mu m emission is contributed, in larger measure than the 24 mu m emission, by dust heated by nonionizing stellar populations, in addition to the ionizing ones, in agreement with previous findings. Two SFR calibrations, one using the 24 mu m emission and the other using a combination of the 24 mu m and H alpha luminosities (Kennicutt and coworkers), are presented. No calibration is presented for the 8 mu m emission because of its significant dependence on both metallicity and environment. The calibrations presented here should be directly applicable to systems dominated by ongoing star formation. C1 Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. NYU, Dept Phys, New York, NY 10003 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London SW7 2AZ, England. Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. RP Calzetti, D (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. EM calzetti@astro.umass.edu OI Bot, Caroline/0000-0001-6118-2985; Draine, Bruce/0000-0002-0846-936X NR 111 TC 520 Z9 520 U1 5 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 SEP 10 PY 2007 VL 666 IS 2 BP 870 EP 895 DI 10.1086/520082 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208FR UT WOS:000249305700021 ER PT J AU Nozawa, T Kozasa, T Habe, A Dwek, E Umeda, H Tominaga, N Maeda, K Nomoto, K AF Nozawa, Takaya Kozasa, Takashi Habe, Asao Dwek, Eli Umeda, Hideyuki Tominaga, Nozomu Maeda, Keiichi Nomoto, Ken'ichi TI Evolution of dust in primordial supernova remnants: can dust grains formed in the ejecta survive and be injected into the early interstellar medium? SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; early universe; shock waves; supernova remnants; supernovae : general ID METAL-POOR STARS; POPULATION-III SUPERNOVAE; CASSIOPEIA-A; EARLY UNIVERSE; ASTROPHYSICAL PLASMAS; INFRARED-EMISSION; DISTANT QUASARS; FORMING CLOUDS; 1ST STARS; GALAXIES AB We investigate the evolution of dust that formed at Population III supernova ( SN) explosions and its processing through the collisions with the reverse shocks resulting from the interaction of the SN ejecta with the ambient medium. In particular, we investigate the transport of the shocked dust within the SNR and its effect on the chemical composition, the size distribution, and the total mass of dust surviving in SNRs. We find that the evolution of the reverse shock, and hence its effect on the processing of the dust, depends on the thickness of the envelope retained by the progenitor star. Furthermore, the transport and survival of the dust grains depend on their initial radius, a(ini), and composition: for Type II SNRs expanding into the ISM with a density of H-n,0 = 1 cm(-3), small grains with a(ini) <= 0.05 mu m are completely destroyed by sputtering in the postshock flow, while grains with (a)ini 0.5-0.2 mu m are trapped into the dense shell behind the forward shock. Very large grains of a(ini) >= 0.2 mu m are ejected into the ISM without decreasing their sizes significantly. We find that the total mass fraction of dust that is destroyed by the reverse shock ranges from 0.2 to 1.0, depending on the energy of the explosion and the density of the ambient ISM. The results of our calculations have significant impact on the abundance pattern of the second-generation stars that form in the dense shell of primordial SNRs. C1 Hokkaido Univ, Grad Sch Sci, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Univ Tokyo, Sch Sci, Dept Astron, Tokyo 1130033, Japan. Max Planck Inst Astrophys, D-85741 Garching, Germany. Univ Tokyo, Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan. RP Nozawa, T (reprint author), Hokkaido Univ, Grad Sch Sci, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. EM tnozawa@mail.sci.hokudai.ac.jp RI Dwek, Eli/C-3995-2012; Nomoto, Ken'ichi/A-4393-2011; Kozasa, Takashi/A-5213-2012 NR 52 TC 152 Z9 152 U1 0 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2007 VL 666 IS 2 BP 955 EP 966 DI 10.1086/520621 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208FR UT WOS:000249305700027 ER PT J AU Dib, R Kaspi, VM Gavriil, FP AF Dib, Rim Kaspi, Victoria M. Gavriil, Fotis P. TI 10 years of RXTE monitoring of the anomalous X-ray pulsar 4U 0142+61: Long-term variability SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (4U 0142+61); stars : neutron; X-rays : stars ID PROPORTIONAL COUNTER ARRAY; SOFT GAMMA REPEATERS; 1RXS J170849.0-400910; NEUTRON-STAR; 1E 2259+586; CHANDRA OBSERVATIONS; SPIN-DOWN; EMISSION; GLITCH; OUTBURST AB We report on 10 years of monitoring of the 8.7 s anomalous X-ray pulsar 4U 0142+ 61 using the Rossi X-Ray Timing Explorer (RXTE). This pulsar exhibited stable rotation from 2000 March until 2006 February; the rms phase residual for a spin-down model, which includes nu , nu, and nu, is 2.3%. We report a possible phase-coherent timing solution valid over a 10 yr span extending back to 1996 March. A glitch may have occurred between 1998 and 2000, but is not required by the existing timing data. The pulse profile has been evolving since 2000. In particular, the dip of emission between its two peaks got shallower between 2002 and 2006, as if the profile were evolving back to its pre-2000 morphology, following an earlier event, which possibly also included the glitch suggested by the timing data. These profile variations are seen in the 2-4 keV band, but not in 6-8 keV. We also detect a slow increase in the pulsed flux between 2002 May and 2004 December, such that it has risen by 36% +/- 3% over 2.6 yr in the 2-10 keV band. The pulsed flux variability and the narrowband pulse profile changes present interesting challenges to aspects of the magnetar model. C1 McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Oak Ridge Associated Univ, Oak Ridge, TN USA. RP Dib, R (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. NR 49 TC 42 Z9 43 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2007 VL 666 IS 2 BP 1152 EP 1164 DI 10.1086/519726 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208FR UT WOS:000249305700042 ER PT J AU Blake, CH Charbonneau, D White, RJ Marley, MS Saumon, D AF Blake, Cullen H. Charbonneau, David White, Russel J. Marley, Mark S. Saumon, Didier TI Multiepoch radial velocity observations of L dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : low-mass; brown dwarfs; techniques : radial velocities ID EXTRASOLAR GIANT PLANETS; BROWN DWARFS; ULTRACOOL DWARFS; ROTATION; SEARCH; MASSES; MODEL; EMISSION; SPECTRA; OBJECTS AB We report on the development of a technique for precise radial velocity measurements of cool stars and brown dwarfs in the near infrared. Our technique is analogous to the iodine (I-2) absorption cell method that has proven so successful in the optical regime. We rely on telluric CH4 absorption features to serve as a wavelength reference, relative to which we measure Doppler shifts of the CO and H2O features in the spectra of our targets. We apply this technique to high-resolution (R approximate to 50; 000) spectra near 2.3 mu m of nine L dwarfs taken with the Phoenix instrument on Gemini South and demonstrate a typical precision of 300 m s(-1). We conduct simulations to estimate our expected precision and show that our performance is currently limited by the signal-to-noise ratio (S/N) of our data. We present estimates of the rotational velocities and systemic velocities of our targets. With our current data we are sensitive to companions with M sin i > 2 M-J in orbits with periods less than 3 days. We identify no companions in our current data set. Future observations with improved S/N should result in radial velocity precision of 100 m s(-1) for L dwarfs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Blake, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Marley, Mark/I-4704-2013; OI Charbonneau, David/0000-0002-9003-484X NR 51 TC 52 Z9 52 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2007 VL 666 IS 2 BP 1198 EP 1204 DI 10.1086/520124 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208FR UT WOS:000249305700046 ER PT J AU Bhattacharyya, S Strohmayer, TE AF Bhattacharyya, Sudip Strohmayer, Tod E. TI Thermonuclear flame spreading on rapidly spinning neutron stars: Indications of the coriolis force? SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : neutron; stars : rotation; X-rays : binaries; X-rays : bursts; X-rays : individual (4U 1636-536, SAX J1808.4-3658) ID X-RAY-BURSTS; HARMONIC CONTENT; RISING PHASE; OSCILLATIONS; FREQUENCY; HZ; PROPAGATION; EVOLUTION; SPECTRA AB Millisecond period brightness oscillations during the intensity rise of thermonuclear X-ray bursts are likely caused by an azimuthally asymmetric, expanding burning region on the stellar surface. The time evolution of the oscillation amplitude during the intensity rise encodes information on how the thermonuclear flames spread across the stellar surface. This process depends on properties of the accreted burning layer, surface fluid motions, and the surface magnetic field structure, and thus can provide insight into these stellar properties. We present two examples of bursts from different sources that show a decrease in oscillation amplitude during the intensity rise. Using theoretical modeling, we demonstrate that the observed amplitude evolution of these bursts is not well described by a uniformly expanding circular burning region. We further show that by including in our model the salient aspects of the Coriolis force (as described by Spitkovsky, Levin, and Ushomirsky) we can qualitatively reproduce the observed evolution curves. Our modeling shows that the evolutionary structure of burst oscillation amplitude is sensitive to the nature of flame spreading, while the actual amplitude values can be very useful to constrain some source parameters. C1 NASA, Goddard Space Flight Ctr, CRESST, Astrophys Sci Div, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Astrophys Sci Div, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Bhattacharyya, S (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM sudip@milkyway.gsfc.nasa.gov; stroh@clarence.gsfcnasa.gov NR 25 TC 9 Z9 9 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2007 VL 666 IS 2 BP L85 EP L88 DI 10.1086/521790 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208GD UT WOS:000249306900007 ER PT J AU Borrero, JM Rubio, LRB Muller, DAN AF Borrero, J. M. Rubio, L. R. Bellot Mueller, D. A. N. TI Flux tubes as the origin of net circular polarization in sunspot penumbrae SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : magnetic fields; sunspots; techniques : polarimetric ID FINE-STRUCTURE; SPECTRAL SIGNATURE; FIELD; FILAMENTS; PROFILES; LINES AB We employ a three-dimensional magnetohydrostatic model of a horizontal flux tube, embedded in a magnetic surrounding atmosphere, to successfully reproduce the azimuthal and center-to-limb variations of the net circular polarization observed in sunspot penumbrae. This success is partly due to the realistic modeling of the interaction between the flux tube and the surrounding magnetic field. C1 NCAR, High Altitude Observ, Boulder, CO 80301 USA. Inst Astrofis Andalucia, CSIC, E-18080 Granada, Spain. NASA, Goddard Space Flight Ctr, European Space Agcy, Greenbelt, MD 20771 USA. RP Borrero, JM (reprint author), NCAR, High Altitude Observ, Boulder, CO 80301 USA. EM borrero@ucar.edu; lbellot@iaa.es; dmueller@esa.nascom.nasa.gov OI Bellot Rubio, Luis Ramon/0000-0001-8669-8857 NR 24 TC 22 Z9 22 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2007 VL 666 IS 2 BP L133 EP L136 DI 10.1086/521923 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208GD UT WOS:000249306900019 ER PT J AU Chiar, JE Ennico, K Pendleton, YJ Boogert, ACA Greene, T Knez, C Lada, C Roellig, T Tielens, AGGM Werner, M Whittet, DCB AF Chiar, J. E. Ennico, K. Pendleton, Y. J. Boogert, A. C. A. Greene, T. Knez, C. Lada, C. Roellig, T. Tielens, A. G. G. M. Werner, M. Whittet, D. C. B. TI The relationship between the optical depth of the 9.7 mu m silicate absorption feature and infrared differential extinction in dense clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared : ISM; ISM : clouds; ISM : molecules ID INTERSTELLAR DUST MODELS; SIZE DISTRIBUTION; DARK CLOUD; GRAINS; SPECTROSCOPY; EMISSION; STARS AB We have examined the relationship between the optical depth of the 9.7 mm silicate absorption feature (tau(9.7)) and the near-infrared color excess E(J - K-s), in the Serpens, Taurus, IC 5146, Chameleon I, Barnard 59, and Barnard 68 dense clouds/cores. Our data set, based largely on Spitzer IRS spectra, spans E(J - K-s) p = 0.3-10 mag (corresponding to visual extinction between about 2 and 60 mag). All lines of sight show the 9.7 mu m silicate feature. Unlike in the diffuse ISM where a tight linear correlation between the 9.7 mu m silicate feature optical depth and the extinction (A(V)) is observed, we find that the silicate feature in dense clouds does not show a monotonic increase with extinction. Thus, in dense clouds, tau(9.7) is not a good measure of total dust column density. With few exceptions, the measured values fall well below the diffuse ISM correlation line for E(J - K-s) > 2 mag (AV > 12 mag). Grain growth via coagulation is a likely cause of this effect. C1 SETI Inst, Mountain View, CA 94043 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. Univ Texas, Austin, TX 78712 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Rensselaer Polytech Inst, Troy, NY 12180 USA. RP Chiar, JE (reprint author), SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. RI Ennico, Kimberly/L-9606-2014 NR 23 TC 51 Z9 51 U1 0 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2007 VL 666 IS 2 BP L73 EP L76 DI 10.1086/521789 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208GD UT WOS:000249306900004 ER PT J AU Wu, YQ Carnell, LA Clark, RL AF Wu, Yiquan Carnell, Lisa A. Clark, Robert L. TI Control of electrospun mat width through the use of parallel auxiliary electrodes SO POLYMER LA English DT Article DE electrospinning; aligned fiber; poly(epsilon-caprolactone) ID UNIAXIALLY ALIGNED ARRAYS; POLYMER NANOFIBERS; FIBERS; SCAFFOLDS; DEPOSITION AB Electrospinning offers a versatile way to produce one-dimensional micrometer or nanometer materials; however, electrospun fibers are typically collected in a random orientation limiting their applications. In the present study, we have expanded upon a technique used to align fibers for control of the fiber distribution during the spinning process through the use of auxiliary counter electrodes. The electrostatic force imposed by the auxiliary electrodes provides a converged electric field, which affords control over the distribution of the fibers on the rotating collector surface. Experimental results demonstrate that the width of electrospun mats can be decreased dramatically when parallel auxiliary electrodes are employed at the collector. There was no apparent difference in the average diameters of the electrospun fibers as a result of the additional auxiliary electrodes, but the fiber distribution density in terms of mat width was greatly improved. Thus, the use of auxiliary counter electrodes at the rotating collectors provides a viable method of converging and controlling the deposition of electrospun fibers. (C) 2007 Elsevier Ltd. All rights reserved. C1 Duke Univ, Pratt Sch Engn, Durham, NC 27708 USA. Duke Univ, Ctr Biol Inspired Mat & Mat Syst, Durham, NC 27708 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Clark, RL (reprint author), Duke Univ, Pratt Sch Engn, Durham, NC 27708 USA. EM rclark@duke.edu NR 32 TC 57 Z9 59 U1 6 U2 31 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0032-3861 J9 POLYMER JI Polymer PD SEP 10 PY 2007 VL 48 IS 19 BP 5653 EP 5661 DI 10.1016/j.polymer.2007.07.023 PG 9 WC Polymer Science SC Polymer Science GA 220MO UT WOS:000250161000024 ER PT J AU Hoang, S Lacombe, C MacDowall, RJ Thejappa, G AF Hoang, S. Lacombe, C. MacDowall, R. J. Thejappa, G. TI Radio tracking of the interplanetary coronal mass ejection driven shock crossed by Ulysses on 10 May 2001 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PLASMA FREQUENCY; THERMAL NOISE; EMISSIONS; INSTRUMENTATION; SPACECRAFT; BURSTS; CME AB We report on the detection of type II radio emission which was observed for more than a day prior to the arrival of an interplanetary shock at Ulysses. We use local spectral emission peaks, computerized from time-averaged intensity spectra of the type II burst, to track the associated emitting shock. In the spectrogram plotted as a function of time and inverse frequency, these peaks appear as elongated clusters of data points, organized in fundamental-harmonic bands and delineating drifting emission features. Least squares linear fittings to identified clusters give straight traces with different slopes. Most of these, when extrapolated to the Sun, are found to converge nearly at the same starting time, allowing determination of the average shock speed. Shortly before the shock crossing, intense Langmuir waves were detected at the electron plasma frequency upstream of the shock. This plasma wave enhancement together with the radio emission observed predominantly at the harmonic of the plasma frequency, all point to the occurrence of the type II radio source region in the upstream electron foreshock. We have accurately substracted the thermal noise background from the observed emission intensity to deduce the type II brightness temperatures at the fundamental and harmonic near the shock crossing. The measured brightness temperature of the type II harmonic emission is found to peak at a value of similar or equal to 3 x 10 13 K just after the shock crossing; just before, the harmonic brightness temperature is similar or equal to 10(12) K and the fundamental brightness temperature similar or equal to 8 x 10 11 K. C1 Observ Paris, Lab Etud Spatiales Instrument Astrophys, Meudon, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Hoang, S (reprint author), Observ Paris, Lab Etud Spatiales Instrument Astrophys, Meudon, France. EM sang.hoang@obspm.fr; catherine.lacombe@obspm.fr; robert.macdowall@nasa.gov; golla@gsfc.nasa.gov RI MacDowall, Robert/D-2773-2012 NR 25 TC 15 Z9 15 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 8 PY 2007 VL 112 IS A9 AR A09102 DI 10.1029/2006JA011906 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 209FE UT WOS:000249373600002 ER PT J AU Taktakishvili, A Kuznetsova, MM Hesse, M Fok, MC Rastatter, L Maddox, M Chulaki, A Gombosi, TI De Zeeuw, DL AF Taktakishvili, A. Kuznetsova, M. M. Hesse, M. Fok, M.-C. Rastaetter, L. Maddox, M. Chulaki, A. Gombosi, T. I. De Zeeuw, D. L. TI Buildup of the ring current during periodic loading-unloading cycles in the magnetotail driven by steady southward interplanetary magnetic field SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID DYNAMIC MAGNETOTAIL; PLASMA SHEET; ACCELERATION; SIMULATION; DECAY; MODEL; IONS AB During prolonged intervals of negative interplanetary magnetic field ( IMF) B-z the magnetosphere often enters a state in which quasi-periodic, large-amplitude oscillations of energetic particle fluxes are observed at the geosynchronous orbit. We use the global magnetosphere MHD code BATS-R-US output during a long period of steady southward IMF Bz to drive the Fok Ring Current Model. Previous simulations of such events demonstrated flat behavior of the energetic particle fluxes after the initial injection. Periodical north/south IMF turning was required to reproduce oscillations in particle fluxes at geosynchronous orbit. In the present study we use a global magnetosphere MHD code that reproduces fast magnetotail reconnection rates observed in kinetic simulations. This results in periodical loading-unloading cycles in the magnetotail even for steady southward Bz and can explain quasi-periodic oscillations of geosynchronous energetic particle fluxes. The total proton energy within geosynchronous orbit exhibits overall growth in time due to quasi-steady convection and oscillates due to injection through inductive electric field caused by multiple dipolarization. The flux oscillation amplitude is stronger in the outer regions of the ring current although the regions close to the geosynchronous orbit experience substantial perturbations as well. C1 NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI USA. RP Taktakishvili, A (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. EM staktak@helio.gsfc.nasa.gov RI Gombosi, Tamas/G-4238-2011; De Zeeuw, Darren/F-3667-2011; Rastaetter, Lutz/D-4715-2012; Kuznetsova, Maria/F-6840-2012; Fok, Mei-Ching/D-1626-2012 OI Gombosi, Tamas/0000-0001-9360-4951; Rastaetter, Lutz/0000-0002-7343-4147; NR 22 TC 13 Z9 13 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 SEP 8 PY 2007 VL 112 IS A9 AR A09203 DI 10.1029/2007JA012317 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 209FE UT WOS:000249373600007 ER PT J AU Klerkx, G AF Klerkx, Greg TI There's no business... SO NEW SCIENTIST LA English DT Article C1 NASA, Washington, DC 20546 USA. RP Klerkx, G (reprint author), NASA, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD SEP 8 PY 2007 VL 195 IS 2620 BP 55 EP 58 DI 10.1016/S0262-4079(07)62283-0 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 208VT UT WOS:000249348000035 ER PT J AU Amaro-Seoane, P Gair, JR Freitag, M Miller, MC Mandel, I Cutler, CJ Babak, S AF Amaro-Seoane, Pau Gair, Jonathan R. Freitag, Marc Miller, M. Coleman Mandel, Ilya Cutler, Curt J. Babak, Stanislav TI Intermediate and extreme mass-ratio inspirals - astrophysics, science applications and detection using LISA SO CLASSICAL AND QUANTUM GRAVITY LA English DT Review ID SUPERMASSIVE BLACK-HOLES; FOKKER-PLANCK MODELS; MONTE-CARLO SIMULATIONS; ANISOTROPIC VELOCITY DISTRIBUTIONS; GLOBULAR-CLUSTER EVOLUTION; GRAVITATIONAL-WAVE SOURCES; TIDAL DISRUPTION EVENTS; YOUNG STAR-CLUSTERS; X-RAY SOURCES; ACTIVE GALACTIC NUCLEI AB Black hole binaries with extreme (greater than or similar to 104 : 1) or intermediate(similar to 10(2)-10(4) : 1) mass ratios are among the most interesting gravitational wave sources that are expected to be detected by the proposed laser interferometer space antenna (LISA). These sources have the potential to tell us much about astrophysics, but are also of unique importance for testing aspects of the general theory of relativity in the strong field regime. Here we discuss these sources from the perspectives of astrophysics, data analysis and applications to testing general relativity, providing both a description of the current state of knowledge and an outline of some of the outstanding questions that still need to be addressed. This review grew out of discussions at a workshop in September 2006 hosted by the Albert Einstein Institute in Golm, Germany. C1 Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Amaro-Seoane, P (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, Muhlenberg 1, D-14476 Potsdam, Germany. EM pau@aei.mpg.de; jrg23@cam.ac.uk; freitag@cam.ac.uk; miller@astro.umd.edu; ilya@caltech.edu; curt.j.cutler@jpl.nasa.gov; stba@aei.mpg.de NR 316 TC 164 Z9 165 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD SEP 7 PY 2007 VL 24 IS 17 BP R113 EP R169 DI 10.1088/0264-9381/24/17/R01 PG 57 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 202NJ UT WOS:000248909000001 ER PT J AU Miller, Y Chaban, GM Zhou, J Asmis, KR Neumark, DM Gerber, RB AF Miller, Yifat Chaban, Galina M. Zhou, Jia Asmis, Knut R. Neumark, Daniel M. Gerber, R. Benny TI Vibrational spectroscopy of (SO(4)(2-))center dot(H(2)O)(n) clusters, n=1-5: Harmonic and anharmonic calculations and experiment SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SELF-CONSISTENT-FIELD; DENSITY-FUNCTIONAL THEORY; AB-INITIO; BIOLOGICAL MOLECULES; GAS-PHASE; EMPIRICAL POTENTIALS; SULFATE DIANION; WAVE-FUNCTIONS; BASIS SETS; ROW ATOMS AB The vibrational spectroscopy of (SO(4)(2-))center dot(H(2)O)(n) is studied by theoretical calculations for n=1-5, and the results are compared with experiments for n=3-5. The calculations use both ab initio MP2 and DFT/B3LYP potential energy surfaces. Both harmonic and anharmonic calculations are reported, the latter with the CC-VSCF method. The main findings are the following: (1) With one exception (H(2)O bending mode), the anharmonicity of the observed transitions, all in the experimental window of 540-1850 cm(-1), is negligible. The computed anharmonic coupling suggests that intramolecular vibrational redistribution does not play any role for the observed linewidths. (2) Comparison with experiment at the harmonic level of computed fundamental frequencies indicates that MP2 is significantly more accurate than DFT/B3LYP for these systems. (3) Strong anharmonic effects are, however, calculated for numerous transitions of these systems, which are outside the present observation window. These include fundamentals as well as combination modes. (4) Combination modes for the n=1 and n=2 clusters are computed. Several relatively strong combination transitions are predicted. These show strong anharmonic effects. (5) An interesting effect of the zero point energy (ZPE) on structure is found for (SO(4)(2-))center dot(H(2)O)(5): The global minimum of the potential energy corresponds to a C(s) structure, but with incorporation of ZPE the lowest energy structure is C(2v), in accordance with experiment. (6) No stable structures were found for (OH(-))center dot(HSO(4)(-))center dot(H(2)O)(n), for n <= 5. (C) 2007 American Institute of Physics. C1 Hebrew Univ Jerusalem, Dept Phys Chem, IL-91904 Jerusalem, Israel. Hebrew Univ Jerusalem, Fritz Haber Res Ctr, IL-91904 Jerusalem, Israel. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Div Chem Sci, Berkeley, CA 94720 USA. Free Univ Berlin, Inst Expt Phys, D-14195 Berlin, Germany. Max Planck Gesell, Fritz Haber Inst, D-14195 Berlin, Germany. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gerber, RB (reprint author), Hebrew Univ Jerusalem, Dept Phys Chem, IL-91904 Jerusalem, Israel. EM benny@fh.huji.ac.il RI Neumark, Daniel/B-9551-2009; Asmis, Knut/N-5408-2014 OI Neumark, Daniel/0000-0002-3762-9473; Asmis, Knut/0000-0001-6297-5856 NR 44 TC 36 Z9 36 U1 0 U2 18 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 J9 J CHEM PHYS JI J. Chem. Phys. PD SEP 7 PY 2007 VL 127 IS 9 AR 094305 DI 10.1063/1.2764074 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 208MP UT WOS:000249323700013 PM 17824737 ER PT J AU Amashukeli, X Pelletier, CC Kirby, JP Grunthaner, FJ AF Amashukeli, Xenia Pelletier, Christine C. Kirby, James P. Grunthaner, Frank J. TI Subcritical water extraction of amino acids from Atacama Desert soils SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID LABELED RELEASE EXPERIMENT; THERMAL REACTION KINETICS; HYDROTHERMAL REACTIONS; ENVIRONMENTAL SOLIDS; HIGH-TEMPERATURE; MARS; LIFE; DECARBOXYLATION; SEARCH; DECOMPOSITION AB Amino acids are considered organic molecular indicators in the search for extant and extinct life in the Solar System. Extraction of these molecules from a particulate solid matrix, such as Martian regolith, will be critical to their in situ detection and analysis. The goals of this study were to optimize a laboratory amino acid extraction protocol by quantitatively measuring the yields of extracted amino acids as a function of liquid water temperature and sample extraction time and to compare the results to the standard HCl vapor- phase hydrolysis yields for the same soil samples. Soil samples from the Yungay region of the Atacama Desert ( Martian regolith analog) were collected during a field study in the summer of 2005. The amino acids ( alanine, aspartic acid, glutamic acid, glycine, serine, and valine) chosen for analysis were present in the samples at concentrations of 1 - 70 parts- per- billion. Subcritical water extraction efficiency was examined over the temperature range of 30 - 325 degrees C, at pressures of 17.2 or 20.0 MPa, and for water- sample contact equilibration times of 0 - 30 min. None of the amino acids were extracted in detectable amounts at 30 degrees C ( at 17.2 MPa), suggesting that amino acids are too strongly bound by the soil matrix to be extracted at such a low temperature. Between 150 degrees C and 250 degrees C ( at 17.2 MPa), the extraction efficiencies of glycine, alanine, and valine were observed to increase with increasing water temperature, consistent with higher solubility at higher temperatures, perhaps due to the decreasing dielectric constant of water. Amino acids were not detected in extracts collected at 325 degrees C ( at 20.0 MPa), probably due to amino acid decomposition at this temperature. The optimal subcritical water extraction conditions for these amino acids from Atacama Desert soils were achieved at 200 degrees C, 17.2 MPa, and a water- sample contact equilibration time of 10 min. C1 Jet Propuls Lab, Pasadena, CA 91109 USA. RP Grunthaner, FJ (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA. EM frank.j.grunthaner@jpl.nasa.gov NR 58 TC 17 Z9 17 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD SEP 7 PY 2007 VL 112 IS G4 AR G04S16 DI 10.1029/2006JG000308 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 209CO UT WOS:000249366200001 ER PT J AU Caceres, L Gomez-Silva, B Garro, X Rodriguez, V Monardes, V Mckay, CP AF Caceres, Luis Gomez-Silva, Benito Garro, Ximena Rodriguez, Violeta Monardes, Vinka McKay, Christopher P. TI Relative humidity patterns and fog water precipitation in the Atacama Desert and biological implications SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID CHILE; LIFE; INSTRUMENT; REGION AB Fog is the most important source of water for native plants and biological soil crusts in the Atacama Desert. Since fog depends upon available moisture, an understanding of climatic patterns is essential to interpret its present-day occurrence and distribution. In this work, temperature and humidity of ambient air and collected fog water in selected sites were studied across a transect from the coast to inland of the Atacama Desert, by using automated outdoor sensors for temperature and relative humidity, and also fog collectors equipped with automated rain gauges to measure collected fog water flow rates. Field measurements were organized to determine fog and collected fog water patterns at three selected sites, namely, Coloso, Inacesa and Yungay in addition to the relative humidity and temperature variation with altitude at Coloso Mountain located within Coloso site. The results show a decreasing trend in the collected fog water flow rates from the coast toward inland locations. Daily thermal oscillations at each site are closely related to fog water collection. At Coloso Mountain, an adiabatic cooling-like effect of the wind ascending its slope was observed preferentially during nighttime. At daytime, occasional distortions observed in the temperature profiles are probably produced by a thermal driven-air convection process along the Coloso Mountain slope heated by solar radiation. The reduction in available water from fog from the coast to the inland site is consistent with the reduction in colonization rate for hypolithic cyanobacteria along this same transect. C1 Univ Antofagasta, Dept Chem Engn, Antofagasta, Chile. Univ Antofagasta, Inst Desierto, Antofagasta, Chile. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA USA. RP Caceres, L (reprint author), Univ Antofagasta, Dept Chem Engn, Antofagasta, Chile. NR 25 TC 10 Z9 10 U1 3 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD SEP 6 PY 2007 VL 112 IS G4 AR G04S14 DI 10.1029/2006JG000344 PG 11 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 209CM UT WOS:000249366000002 ER PT J AU Connon, SA Lester, ED Shafaat, HS Obenhuber, DC Ponce, A AF Connon, Stephanie A. Lester, Elizabeth D. Shafaat, Hannah S. Obenhuber, Donald C. Ponce, Adrian TI Bacterial diversity in hyperarid Atacama Desert soils SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID FRANKIA STRAINS; NORTHERN CHILE; RUBROBACTER-RADIOTOLERANS; ACINETOBACTER-BAUMANNII; DESICCATION TOLERANCE; NITRATE DEPOSITS; ROOT-NODULES; MARS; PROKARYOTES; PLANTS AB Surface and subsurface soil samples analyzed for this investigation were collected from the hyperarid Yungay region in the Atacama Desert, Chile. This report details the bacterial diversity derived from DNA and PLFA extracted directly from these extremely desiccated soils. Actinobacteria, Proteobacteria, Firmicutes and TM7 division bacteria were detected. Ninety- four percent of the 16S rRNA genes cloned from these soils belong to the Actinobacteria phylum, and the majority of these were most closely related to the genus Frankia. A 24- hour water activity (a(w)) time course showed a diurnal cycle that peaked at 0.52 in the early predawn hours, and ranged from 0.01 - 0.08 during the day. All measured water activity values were below the levels required for microbial growth or enzyme activity. Total organic carbon ( TOC) concentrations were above the limit of detection and below the limit of quantification (i.e., 200 mu g/g < TOC < 1000 mu g/g), and phospholipid fatty acid ( PLFA) concentrations ranged from 2 x 10(5) to 7 x 10(6) cell equivalents per gram of soil. Soil extracts analyzed for culturable biomass yielded mostly no growth on R2A media; the highest single extract yielded 47 colony forming units ( CFU) per gram of soil. C1 Jet Propuls Lab, Pasadena, CA 91109 USA. RP Connon, SA (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA. RI Connon, Stephanie/K-1959-2012 NR 57 TC 56 Z9 58 U1 6 U2 43 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD SEP 6 PY 2007 VL 112 IS G4 AR G04S17 DI 10.1029/2006JG000311 PG 9 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 209CM UT WOS:000249366000001 ER PT J AU Davydov, VA Rakhmanina, AV Rols, S Agafonov, V Pulikkathara, MX Wal, RLV Khabashesku, VN AF Davydov, V. A. Rakhmanina, A. V. Rols, S. Agafonov, V. Pulikkathara, M. X. Wal, R. L. Vander Khabashesku, V. N. TI Size-dependent phase transition of diamond to graphite at high pressures SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID ONION-LIKE CARBON; CHEMICAL VAPOR-DEPOSITION; X-RAY-DIFFRACTION; RAMAN-SPECTRUM; MOLECULAR-DYNAMICS; HIGH-TEMPERATURE; HEAT-TREATMENT; ARGON AMBIENT; TRANSFORMATION; CLUSTERS AB Size-dependent phase transition of nanosize diamond particles (NDPs) to graphite was found in the course of studies of high pressure high temperature (HPHT) induced transformations of NDPs at 8 GPa and in the temperature range of 873-1623 K. Analysis of the products of HPHT treatment of powder NDPs (with the mean size of 4.5 nm) by X-ray diffraction (XRD), scanning (SEM) and transmission electron (TEM) microscopies, and Raman spectroscopy have shown that at 8 GPa the increase of the treatment temperature results in a gradual enlargement of NDPs. According to XRD data, the temperature increase from 873 to 1473 K at the treatment time of 60 s gives rise to NDP mean size enlargement from initial 4.5 to 8.8 nm. However, the largest NDPs can reach the sizes of 13.5-14.0 nm at 1473 K, as measured directly from TEM images. At 1623 K, size-dependent phase transition of diamond to graphite has been observed. By applying the Arrenius equation to the particle mean size versus treatment temperature plot, activation energy for the diamond solid phase growth at 8 GPa was calculated to be 112 8 kJ/mol. The critical size of NDP corresponding to the point of phase transition at 8 GPa and 1623 K was estimated to be similar to 18 run. The likely effect of the size-dependent diamond-to-graphite phase transition on the process of diamond synthesis and, in particular, the problem of formation of critical seeds for crystal growth of macroscale diamond are discussed in the paper. C1 RAS, LF Vereshchagin Inst High Pressure Phys, Moscow 142190, Russia. Inst Laue Langevin, F-38042 Grenoble, France. Univ Tours, CEA, CNRS, UMR,CEA 6157,LRC,M01, F-37200 Tours, France. Richard E Smalley Inst Nanoscale Sci & Technol, Houston, TX 77005 USA. NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH 44135 USA. RP Davydov, VA (reprint author), RAS, LF Vereshchagin Inst High Pressure Phys, Moscow 142190, Russia. EM vdavydov@hppi.troitsk.r-u; khval@rice.edu RI ROLS, Stephane/A-1609-2013; Davydov, Valery/P-5673-2015 OI ROLS, Stephane/0000-0002-9892-816X; Davydov, Valery/0000-0002-8702-0340 NR 46 TC 10 Z9 12 U1 2 U2 22 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1932-7447 J9 J PHYS CHEM C JI J. Phys. Chem. C PD SEP 6 PY 2007 VL 111 IS 35 BP 12918 EP 12925 DI 10.1021/jp073576k PG 8 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 206FS UT WOS:000249169900009 ER PT J AU Meerkoetter, R Zinner, T AF Meerkoetter, Ralf Zinner, Tobias TI Satellite remote sensing of cloud base height for convective cloud fields: A case study SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EFFECTIVE RADIUS; RETRIEVAL AB A method is proposed for estimating base heights of convective clouds from satellite data. The approach takes advantage of the fact that convective water clouds appear as geometrically and optically thin clouds near an approximately constant condensation level in their earliest stage of growth and that deriving geometrical thicknesses for such thin clouds is less error prone. Striking is the fact that the method also provides the base height for clouds with large vertical extensions and high optical thicknesses. The method has been applied to NOAA/AVHRR data of 20 selected cloud scenes. For an evaluation satellite retrieved cloud base heights have been compared to surface ceilometer measurements at the same time. First results are encouraging. The standard deviation of the differences between satellite and ceilometer measurements is +/- 369m with no systematic bias. C1 DLR, Deutsches Zentrum Luft & Raumfahrt, Inst Phys atmosphare, D-82234 Oberpfaffenhofen, Wessling, Germany. Nasa Goddard Space Flight Ctr, Greenbelt, MD USA. RP Meerkoetter, R (reprint author), DLR, Deutsches Zentrum Luft & Raumfahrt, Inst Phys atmosphare, D-82234 Oberpfaffenhofen, Wessling, Germany. EM ralf.meerkoetter@dlr.de; tobias.zinner@dlr.de RI Zinner, Tobias/B-8991-2013 NR 13 TC 3 Z9 3 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 5 PY 2007 VL 34 IS 17 AR L17805 DI 10.1029/2007GL030347 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 209BU UT WOS:000249364000001 ER PT J AU Ziemke, JR Chandra, S Schoeberl, MR Froidevaux, L Read, WG Levelt, PF Bhartia, PK AF Ziemke, J. R. Chandra, S. Schoeberl, M. R. Froidevaux, L. Read, W. G. Levelt, P. F. Bhartia, P. K. TI Intra-seasonal variability in tropospheric ozone and water vapor in the tropics SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MADDEN-JULIAN OSCILLATION; OUTGOING LONGWAVE RADIATION; INTRASEASONAL OSCILLATIONS; ZONAL WIND; EL-NINO; ATLANTIC AB Nearly two years of tropospheric O-3 and H2O data from the Aura Ozone Monitoring Instrument (OMI) and Microwave Limb Sounder (MLS) instruments are analyzed to study the characteristics of intra-seasonal oscillation (ISO) of 20-100 day periods. The analysis shows the presence of ISO signals in O-3 and H2O throughout much of the tropics including the north Atlantic not shown in previous studies. ISO variability west of the dateline appears as a manifestation of eastward propagation of the Madden-Julian Oscillation (MJO). Time series of tropospheric O-3 and H2O are negatively correlated throughout much of the tropics, and mostly over ocean. This suggests lofting of air from convection as a basic driving mechanism, with convection transporting low amounts of O-3 and high amounts of H2O upwards from the boundary layer. ISO/MJO related changes in O-3 and H2O are a major source of variability and often exceed 25% of background concentrations. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, Baltimore, MD USA. NASA, Jet Propuls Lab, Greenbelt, MD USA. Royal dutch Meterol Inst, NL-3730 AE De Bilt, Netherlands. RP Ziemke, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ziemke@jwocky.gsfc.nasa.gov RI Bhartia, Pawan/A-4209-2016 OI Bhartia, Pawan/0000-0001-8307-9137 NR 28 TC 11 Z9 12 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 5 PY 2007 VL 34 IS 17 AR L17804 DI 10.1029/2007GL030965 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 209BU UT WOS:000249364000007 ER PT J AU Evans, D Pottier, C Fletcher, R Hensley, S Tapley, I Milne, A Barbetti, M AF Evans, Damian Pottier, Christophe Fletcher, Roland Hensley, Scott Tapley, Ian Milne, Anthony Barbetti, Michael TI A comprehensive archaeological map of the world's largest preindustrial settlement complex at Angkor, Cambodia SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE archaeology; geographic information systems; remote sensing; southeast Asia; urbanism AB The great medieval settlement of Angkor in Cambodia [9th-16th centuries Common Era (CE)] has for many years been understood as a "hydraulic city," an urban complex defined, sustained, and ultimately overwhelmed by a complex water management network. Since the 1980s that view has been disputed, but the debate has remained unresolved because of insufficient data on the landscape beyond the great temples: the broader context of the monumental remains was only partially understood and had not been adequately mapped. Since the 1990s, French, Australian, and Cambodian teams have sought to address this empirical deficit through archaeological mapping projects by using traditional methods such as ground survey in conjunction with advanced radar remote-sensing applications in partnership with the National Aeronautics and Space Administration (NASA)/Jet Propulsion Laboratory (JPL). Here we present a major outcome of that research: a comprehensive archaeological map of greater Angkor, covering nearly 3,000 km(2), prepared by the Greater Angkor Project (GAP). The map reveals a vast, low-density settlement landscape integrated by an elaborate water management network covering > 1,000 km(2), the most extensive urban complex of the preindustrial world. It is now clear that anthropogenic changes to the landscape were both extensive and substantial enough to have created grave challenges to the long-term viability of the settlement. C1 Univ Sydney, Archaeol Comp Lab, Sydney, NSW 2006, Australia. Univ Sydney, Dept Archaeol, Sydney, NSW 2006, Australia. Ecole Francaise Extreme Orient, Siem Reap, Cambodia. NASA, Jet Prop Lab, Pasadena, CA 91109 USA. Horizon Geosci Consulting, Perth, WA 6020, Australia. Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. Univ Queensland, Sch Phys Sci, Brisbane, Qld 4072, Australia. RP Evans, D (reprint author), Univ Sydney, Archaeol Comp Lab, Madsen Bldg F09, Sydney, NSW 2006, Australia. EM evans@aci.arts.usyd.edu.au NR 32 TC 65 Z9 68 U1 5 U2 22 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 SEP 4 PY 2007 VL 104 IS 36 BP 14277 EP 14282 DI 10.1073/pnas.0702525104 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 208QF UT WOS:000249333600020 PM 17717084 ER PT J AU Jain, P Raj, SV Hemker, KJ AF Jain, Plyush Raj, Sai V. Hemker, K. J. TI Characterization of NiCrAlY coatings for a high strength, high conductivity GRCop-84 copper alloy SO ACTA MATERIALIA LA English DT Article DE coatings; tension test; adhesion; finite element modeling ID THERMAL BARRIER COATINGS; ALUMINIDE BOND COAT; SUBSTRATE ADHESION; FILMS AB NiCrAlY top coats are currently being considered as environmental protective coatings for copper alloy liners in rocket engine combustion chambers of reusable launch vehicles. The microstructure and mechanical properties of this top coat sprayed on GRCop-84 have been characterized as a function of thermal cycling between 298 and 873 K and no obvious degradation was observed. Interfacial microsample tensile tests developed to measure coating adhesion to the substrate revealed that the interfaces were stronger than the substrate in both the as-received and thermal cycled conditions. Finite element modeling was used to analyze the stresses in the microsamples and verify the strength of the interfaces. The formation of depleted zones, devoid of Cr2Nb particles, was associated with plasma arc cleaning in a minority of the samples prepared for this study, and the presence of these depleted zones has been found to significantly decrease the adhesion of the NiCrAlY coating and to change the failure mode in thermal cycled specimens. (C) 2007 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 Johns Hopkins Univ, Dept Mech Engn, Baltimore, MD 21218 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Hemker, KJ (reprint author), Johns Hopkins Univ, Dept Mech Engn, Baltimore, MD 21218 USA. EM hemker@jhu.edu RI Hemker, Kevin/A-3315-2010 NR 31 TC 4 Z9 4 U1 2 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 J9 ACTA MATER JI Acta Mater. PD SEP PY 2007 VL 55 IS 15 BP 5103 EP 5113 DI 10.1016/j.actamat.2007.05.044 PG 11 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 216RG UT WOS:000249896100017 ER PT J AU Hou, PY Paulikas, AP Veal, BW Smialek, JL AF Hou, P. Y. Paulikas, A. P. Veal, B. W. Smialek, J. L. TI Thermally grown Al(2)O(3) on a H(2)-annealed Fe(3)Al alloy: Stress evolution and film adhesion SO ACTA MATERIALIA LA English DT Article DE oxidation; stresses; adhesion; interface segregation; buckling ID HIGH-TEMPERATURE OXIDATION; OXIDE SCALE ADHERENCE; ALUMINA SCALES; SULFUR SEGREGATION; TRANSIENT OXIDATION; REACTIVE ELEMENT; BEHAVIOR; IRON; KINETICS; YTTRIUM AB Stress evolution in Al(2)O(3) films grown on a Fe(3)Al-based alloy, with or without a prior H(2)-anneal heat treatment, was followed in situ with a synchrotron X-ray source at 1000 and 1100 degrees C and during cooling. These results are complimented by studies of oxidation kinetics, the scale/alloy interfacial chemistry, and the oxide, alloy and interface microstructures. The H(2)-anneal reduced the sample sulfur impurity to less than 1 ppm, significantly improved scale adhesion, maintained a planar scale/alloy interface, but did not demonstrably affect the oxidation rate or the growth stress development. On the untreated alloy, interface wrinkling was a major stress relief mechanism, but for the H(2)-annealed samples it was oxide creep with contribution from alloy grain boundary sliding. The interface strength and the extent of oxide spallation were closely related to the amount of sulfur segregated at the interface. (c) 2007 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 Univ Calif Berkeley, Lawrence Berkeley Lab, Div Mat Sci, Berkeley, CA 94720 USA. Argonne Natl Lab, Argonne, IL 60439 USA. NASA, Glen Res Ctr, Cleveland, OH 44135 USA. RP Hou, PY (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Div Mat Sci, 1 Cyclotron Rd, Berkeley, CA 94720 USA. EM pyhou@lbl.gov NR 60 TC 21 Z9 21 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 J9 ACTA MATER JI Acta Mater. PD SEP PY 2007 VL 55 IS 16 BP 5601 EP 5613 DI 10.1016/j.actamat.2007.06.018 PG 13 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 211SC UT WOS:000249542600029 ER PT J AU Choudhari, MM Khorrami, MR AF Choudhari, Meelan M. Khorrami, Mehdi R. TI Effect of three-dimensional shear-layer structures on slat cove unsteadiness SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 44th Aerospace Sciences Meeting and Exhibit CY JAN 09-12, 2006 CL Reno, NV SP AIAA ID PLANE MIXING LAYER; HIGH-LIFT; TRAILING-EDGE; PREDICTION; NOISE; FLOW; COMPUTATIONS AB Numerical simulations are used to investigate the local and global dynamics of large-scale, three-dimensional vorticity structures within the free shear layer originating from the slat cusp of a multielement airfoil configuration. Results indicate that accounting for the local three-dimensionality of flow fluctuations leads to substantially improved agreement between the computed unsteady near-field solution and wind tunnel measurements based on particle image velocimetry. Analysis of simulation data indicates the potential significance of high intensity turbulent fluctuations near the reattachment location along the slat lower surface toward the generation of broadband slat noise. The computed acoustic characteristics, in terms of the frequency spectrum and spatial distribution within short distances from the slat, resemble the previously reported, subscale measurements of slat noise. C1 NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. RP Choudhari, MM (reprint author), NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 NR 62 TC 10 Z9 10 U1 3 U2 7 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD SEP PY 2007 VL 45 IS 9 BP 2174 EP 2186 DI 10.2514/1.24812 PG 13 WC Engineering, Aerospace SC Engineering GA 210JE UT WOS:000249451700007 ER PT J AU Sivathanu, Y Limt, J Reinhart, LE Bowman, RC AF Sivathanu, Yudaya Limt, Jongmook Reinhart, Laurence E. Bowman, Robert C., Jr. TI Structure of plumes from burning aluminized propellant estimated using fan beam emission tomography SO AIAA JOURNAL LA English DT Article ID ROCKET PLUME; IR EMISSION; RADIATION; TEMPERATURES; FLAME; FLOW AB Fan beam emission tomography in the 1-5-mu m band is used to estimate the structure of a solid rocket propellant plume. Fan beam emission tomography consists of two components. The first is a pair of orthogonal high-speed imaging spectrometers and scanners that measures the spectral radiation intensities from 1.3 to 4.8 mu m at 256 view angles. The second is a robust deconvolution algorithm that estimates the structure of the plume from the spectral radiation intensity measurements. The deconvolution algorithm is based on the maximum likelihood estimation method in conjunction with a linearized radiative transfer equation. The radiation intensity measurements were completed in a series of burns using 2.5-cm-diam by 1.25-cm-long strands of aluminized solid rocket composite propellant. In general, the aluminum diffusion-flame particulate temperatures in the plume are much higher than the gas temperatures. The gaseous combustion product concentrations are much lower in the middle of the plume than at the outer edges. This indicates a diffusion-flame-type structure for the plume, caused by the fact that the composite solid rocket propellant is fuel-rich. The results indicate that reliable plume-structure measurements can be obtained using fan beam emission tomography. C1 En Urga Inc, W Lafayette, IN 47906 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP Sivathanu, Y (reprint author), En Urga Inc, W Lafayette, IN 47906 USA. OI Bowman, Robert/0000-0002-2114-1713 NR 18 TC 3 Z9 3 U1 1 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD SEP PY 2007 VL 45 IS 9 BP 2259 EP 2266 DI 10.2514/1.28742 PG 8 WC Engineering, Aerospace SC Engineering GA 210JE UT WOS:000249451700015 ER PT J AU Martinez, OA Sankar, BV Haftka, RT Bapanapalli, SK Blosser, ML AF Martinez, Oscar A. Sankar, Bhavani V. Haftka, Raphael T. Bapanapalli, Satish K. Blosser, Max L. TI Micromechanical analysis of composite corrugated-core sandwich panels for integral thermal protection systems SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 47th Structures, Structural Dynamics, and Materials Conference CY MAY 01-04, 2006 CL Newport, RI SP AIAA, ASME, ASCE, AHS, ASC ID SHEAR STIFFNESS AB A composite corrugated-core sandwich panel was investigated as a potential candidate for an integral thermal protection system. This multifunctional integral thermal protection system concept can protect the space vehicle from extreme reentry temperatures, and possess load-carrying capabilities. The corrugated core is composed of two, thin, flat sheets that are separated by two inclined plates. Advantages of this new integral thermal protection system concept are discussed. The sandwich structure is idealized as an equivalent orthotropic thick-plate continuum. The extensional stiffness matrix [A], coupling stiffness matrix [B], bending stiffness [D], and the transverse shear stiffness terms A(44) and A(55) were calculated using an energy approach. Using the shear-deformable plate theory, a closed-form solution of the plate response was derived. The variation of plate stiffness and maximum plate deflection due to changing the web angle are discussed. The calculated results, which require significantly less computational effort and time, agree well with the three-dimensional finite element analysis. This study indicates that panels with rectangular webs resulted in a weak extensional, bending, and A55 stiffness and that the center plate deflection was minimum for a triangular corrugated core. The micromechanical analysis procedures developed in this study were used to determine the stresses in each component of the sandwich panel (face and web) due to a uniform pressure load. C1 Univ Florida, Gainesville, FL 32611 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. NASA, Langley Res Ctr, Washington, DC 20546 USA. RP Martinez, OA (reprint author), Univ Florida, Gainesville, FL 32611 USA. RI Sankar, Bhavani/F-5193-2011; OI Sankar, Bhavani/0000-0002-4556-1982 NR 19 TC 24 Z9 30 U1 1 U2 9 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD SEP PY 2007 VL 45 IS 9 BP 2323 EP 2336 DI 10.2514/1.26779 PG 14 WC Engineering, Aerospace SC Engineering GA 210JE UT WOS:000249451700021 ER PT J AU Andrews, RJ AF Andrews, R. J. TI Nanotechnology for neurosurgery SO AMINO ACIDS LA English DT Meeting Abstract C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0939-4451 J9 AMINO ACIDS JI Amino Acids PD SEP PY 2007 VL 33 IS 3 BP XVIII EP XIX PG 2 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 206UH UT WOS:000249207900055 ER PT J AU Cassell, AM Li, J Nguyen-Vu, TDB Chen, H Koehne, J Andrews, R Meyyappan, M AF Cassell, A. M. Li, J. Nguyen-Vu, T.-D. B. Chen, H. Koehne, J. Andrews, R. Meyyappan, M. TI Multiwalled carbon nanotubes: interconnecting solid-state electronics with biosystems SO AMINO ACIDS LA English DT Meeting Abstract C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0939-4451 J9 AMINO ACIDS JI Amino Acids PD SEP PY 2007 VL 33 IS 3 BP XX EP XX PG 1 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 206UH UT WOS:000249207900059 ER PT J AU Stern, J Wang, Y Gu, B Newman, J AF Stern, J. Wang, Y. Gu, B. Newman, J. TI Distribution and turnover of carbon in natural and constructed wetlands in the Florida Everglades SO APPLIED GEOCHEMISTRY LA English DT Article ID DISSOLVED ORGANIC-CARBON; HUMIC SUBSTANCES; METAL SPECIATION; MATTER; C-14; WATER; ACCUMULATION; BINDING; SURFACE; ACCRETION AB Stable and radiocarbon isotopic contents of dissolved organic C (DOC), dissolved inorganic C (DIC), particulate organic C (POC) and plants were used to examine the source and turnover rate of C in natural and constructed wetlands in the Florida Everglades. DOC concentrations decreased, with P concentrations, along a water quality gradient from the agriculturally impacted areas in the northern Everglades to the more pristine Everglades National Park. delta C-13 values of DOC in the area reflect contributions of both wetland vegetation and sugarcane from agriculture. Radiocarbon ages of DOC, POC and DIC in the Everglades ranged from 2.01 ka BP to ">modern". The old C-14 ages of DOC and POC were found in impacted areas near the Everglades Agricultural Area (EAA) in the northern Everglades. In contrast, DOC and POC in pristine marsh areas had near modern or ">modern" C-14 ages. These data indicate that a major source of POC and DOC in impacted areas is the degradation of historic peat deposits in the EAA. In the pristine areas of the marsh, DOC represents a mix of modern and historic C sources, whereas POC comes from modern primary production as indicated by positive A C-14 values, suggesting that DOC is transported farther away from its source than POC. High A C-14 values of DIC indicate that dissolution of limestone bedrock is not a significant source of DIC in the Everglades wetlands. As a restored wetland moves towards its "original" or "natural" state, the C-14 signatures of DOC should approach that of modern atmosphere. In addition, measurements of concentration and C isotopic composition of DOC in two small constructed wetlands (i.e., test cells) indicate that these freshwater wetland systems contain a labile DOC pool with rapid turnover times of 26-39 days and that the test cells are overall net sinks of DOC. (C) 2007 Elsevier Ltd. All rights reserved. C1 Florida State Univ, Dept Geol Sci, Tallahassee, FL 32306 USA. Natl High Magnet Field Lab, Tallahassee, FL 32306 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. S Florida Water Management Dist, Everglades Div, W Palm Beach, FL 33406 USA. RP Wang, Y (reprint author), Florida State Univ, Dept Geol Sci, Tallahassee, FL 32306 USA. EM ywang@magnet.fsu.edu RI Stern, Jennifer/E-3135-2012 OI Stern, Jennifer/0000-0002-0162-8807 NR 36 TC 26 Z9 29 U1 3 U2 24 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0883-2927 J9 APPL GEOCHEM JI Appl. Geochem. PD SEP PY 2007 VL 22 IS 9 BP 1936 EP 1948 DI 10.1016/j.apgeochem.2007.04.007 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 216VH UT WOS:000249906600007 ER PT J AU Coble, K Bonamente, M Carlstrom, JE Dawson, K Hasler, N Holzapfel, W Joy, M LaRoque, S Marrone, DP Reese, ED AF Coble, K. Bonamente, M. Carlstrom, J. E. Dawson, K. Hasler, N. Holzapfel, W. Joy, M. LaRoque, S. Marrone, D. P. Reese, E. D. TI Radio sources toward galaxy clusters at 30 ghz SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; galaxies : clusters : general; radio continuum : galaxies ID MEDIUM-SENSITIVITY SURVEY; ZELDOVICH EFFECT MEASUREMENTS; RAY BRIGHTEST CLUSTERS; ALL-SKY SURVEY; X-RAY; WARPS SURVEY; OPTICAL SPECTROSCOPY; MICROWAVE-ANISOTROPY; ABELL CLUSTERS; HIGH-FREQUENCY AB Extragalactic radio sources are a significant contaminant in cosmic microwave background and Sunyaev-Zel'dovich effect experiments. Deep interferometric observations with the BIMA and OVRO arrays are used to characterize the spatial, spectral, and flux distributions of radio sources toward massive galaxy clusters at 28.5 GHz. We compute counts of millijansky source fluxes from 89 fields centered on known massive galaxy clusters and 8 noncluster fields. We find that source counts in the inner regions of the cluster fields (within 0.5' of the cluster center) are a factor of 8.9(-2.8)(+4.3) times higher than counts in the outer regions of the cluster fields ( radius greater than 0.5'). Counts in the outer regions of the cluster fields are, in turn, a factor of 3.3(-1.8)(+4.1) greater than those in the noncluster fields. Counts in the noncluster fields are consistent with extrapolations from the results of other surveys. We compute the spectral indices of millijansky sources in the cluster fields between 1.4 and 28.5 GHz and find a mean spectral index of alpha = 0.66 with an rms dispersion of 0.36, where flux S proportional to v(-alpha). The distribution is skewed, with a median spectral index of 0.72 and 25th and 75th percentiles of 0.51 and 0.92, respectively. This is steeper than the spectral indices of stronger field sources measured by other surveys. C1 Chicago State Univ, Dept Chem & Phys, Chicago, IL 60628 USA. Alder Planetarium & Astron Museum, Chicago, IL 60605 USA. Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmolog Phys, Chicago, IL 60637 USA. NASA, George C Marshall Space Flight Ctr, NSSTC, Dept Space Sci, Huntsville, AL 35812 USA. Univ Alabama, Dept Phys, Huntsville, AL 35805 USA. Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. RP Coble, K (reprint author), Chicago State Univ, Dept Chem & Phys, 9501 S King Dr, Chicago, IL 60628 USA. EM coble@oddjob.uchicago.edu RI Holzapfel, William/I-4836-2015; OI Marrone, Daniel/0000-0002-2367-1080 NR 68 TC 43 Z9 43 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2007 VL 134 IS 3 BP 897 EP 905 DI 10.1086/519973 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QD UT WOS:000249058200001 ER PT J AU Norton, AJ Mukai, K AF Norton, A. J. Mukai, K. TI A precessing accretion disc in the intermediate polar XY Arietis? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : novae; cataclysmic variables; X-rays : binaries; stars : magnetic fields; stars : binaries : eclipsing; stars : individual : XY Ari; accretion; accretion discs ID MAGNETIC CATACLYSMIC VARIABLES; WHITE-DWARFS; MOLECULAR CLOUD; RAY BINARIES; TV COLUMBAE; LYNDS 1457; PERIODICITIES; PHOTOMETRY; OUTBURSTS; DISCOVERY AB Context. XY Ari is the only intermediate polar to show deep X-ray eclipses of its white dwarf. Previously published observations with Ginga and Chandra have also revealed a broad X-ray orbital modulation, roughly antiphased with the eclipse, and presumed to be due to absorption in an extended structure near the edge of an accretion disc. The X-ray pulse profile is generally seen to be double-peaked, although a single-peaked pulse was seen by RXTE during an outburst in 1996. Aims. We intended to investigate the cause of the broad orbital modulation in XY Ari to better understand the accretion flow in this system and other intermediate polars. Methods. We observed XY Ari with RXTE and analysed previously unpublished archival observations of the system made with ASCA and XMM-Newton. These observations comprise six separate visits and span about ten years. Results. The various X-ray observations show that the broad orbital modulation varies in phase and significance, then ultimately disappears entirely in the last few years. In addition, the X-ray pulse profile shows variations in depth and shape, and in the recent RXTE observations displays no evidence for changes in hardness ratio. Conclusions. The observed changes indicates that both the pulse profile and the orbital modulation are solely due to geometrical effects at the time of the RXTE observations, rather than phase-dependent variations in photoelectric absorption as seen previously. We suggest that this is evidence for a precessing, tilted accretion disc in this system. The precession of the disc moves structures out of our line of sight both at its outer edge ( changing the orbital modulation) and at its inner edge where the accretion curtains are anchored ( changing the pulse profile). C1 Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. NASA, Xray Astrophys Lab, GSFC, CRESST, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Norton, AJ (reprint author), Open Univ, Dept Phys & Astron, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM A.J.Norton@open.ac.uk; mukai@milkyway.gsfc.nasa.gov NR 33 TC 6 Z9 6 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2007 VL 472 IS 1 BP 225 EP 232 DI 10.1051/0004-6361:20077761 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214SK UT WOS:000249758200024 ER PT J AU Kasper, M Apai, D Janson, M Brandner, W AF Kasper, M. Apai, D. Janson, M. Brandner, W. TI A novel L-band imaging search for giant planets in the Tucana and beta Pictoris moving groups SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrometry; stars : late-type; stars : low mass, brown dwarfs; stars : binaries : general; instrumentation : high angular resolution ID ADAPTIVE OPTICS SYSTEM; EXTRASOLAR PLANETS; AU MICROSCOPII; BROWN DWARFS; COMPANION; STARS; DISK; ASSOCIATIONS; HOROLOGIUM; LUMINOSITY AB Context. Direct imaging using various techniques for suppressing the stellar halo nowadays can achieve the contrast levels required to detect and characterize the light of substellar companions at orbital distances greater than a few astronomical units from their host stars. The method nicely complements the radial velocity surveys that provide evidence that giant extrasolar planets in close-in orbits are relatively common. Aims. The paper presents results from a small survey of 22 young, nearby stars that was designed to detect substellar companions and ultimately giant extrasolar planets down to Jupiter masses. The targets are members of the Tucana and beta Pictoris moving groups, apart from the somewhat older star HIP 71395, which has a radial velocity trend suggesting a massive planet in large orbit. Methods. The survey was carried out in the L-band using adaptive optics-assisted imaging with NAOS-CONICA (NACO) at the VLT. The chosen observation wavelength is well-suited to searching for close companions around young stars and it delivers unprecedented detection limits. The presented technique reaches some of the best sensitivities as of today and is currently the most sensitive method for the contrast-limited detection of substellar companions that are cooler than about 1000 K. Results. The companion to 51 Eri, GJ 3305, was found to be a very close binary on an eccentric orbit. No substellar companions were found around the target stars, although the method permitted companions to be detected down to a few Jupiter masses at orbital distances typically of 5 astronomical units. A planet with a mass >= 1 M(Jup) at distances >= 5AU around AU Mic can be excluded at the time of our observations. The absence of detected planets sets constraints on the frequency distribution and maximum orbital distance of giant exoplanets. For example, a radial distribution power law index of 0.2 in combination with a maximum orbital radius exceeding 30 AU can be rejected at a 90% confidence level. Conclusions. C1 European So Observ, D-85748 Garching, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NASA, Astrobiol Inst, Washington, DC 20546 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Calif Los Angeles, Div Astron, Los Angeles, CA 90095 USA. RP Kasper, M (reprint author), European So Observ, Karl-Schwarzschild-Str 2, D-85748 Garching, Germany. EM mkasper@eso.org NR 34 TC 85 Z9 85 U1 3 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2007 VL 472 IS 1 BP 321 EP U203 DI 10.1051/0004-6361:20077646 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214SK UT WOS:000249758200038 ER PT J AU Segura, A Meadows, VS Kasting, JF Crisp, D Cohen, M AF Segura, A. Meadows, V. S. Kasting, J. F. Crisp, D. Cohen, M. TI Abiotic formation of O-2 and O-3 in high-CO2 terrestrial atmospheres SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrobiology; infrared : general; ultraviolet : stars ID COLLISION-INDUCED ABSORPTION; NEOPROTEROZOIC SNOWBALL EARTH; YOUNG SUN; PLANETARY-ATMOSPHERES; OXYGEN CONCENTRATION; OXIDATION-STATE; HABITABLE ZONES; UV-RADIATION; WATER-VAPOR; EVOLUTION AB Context. Previous research has indicated that high amounts of ozone (O-3) and oxygen ( O-2) may be produced abiotically in atmospheres with high concentrations of CO2. The abiotic production of these two gases, which are also characteristic of photosynthetic life processes, could pose a potential " false- positive" for remote- sensing detection of life on planets around other stars. We show here that such false positives are unlikely on any planet that possesses abundant liquid water, as rainout of oxidized species onto a reduced planetary surface should ensure that atmospheric H-2 concentrations remain relatively high, and that O-2 and O-3 remain low. Aims. Our gool is to determine the amount of O-3 and O-2 formed in a high CO2 atmosphere for a habitable planet without life. Methods. We use a photochemical model that considers hydrogen ( H-2) escape and a detailed hydrogen balance to calculate the O-2 and O-3 formed on planets with 0.2 of CO2 around the Sun, and 0.02, 0.2 and 2 bars of CO2 around a young Sun- like star with higher UV radiation. The concentrations obtained by the photochemical model were used as input in a radiative transfer model that calculated the spectra of the modeled planets. Results. The O-3 and O-2 concentrations in the simulated planets are extremely small, and unlikely to produce a detectable signature in the spectra of those planets. Conclusions. With a balanced hydrogen budget, and for planets with an active hydrological cycle, abiotic formation of O-2 and O-3 is unlikely to create a possible false positive for life detection in either the visible/ near- infrared or mid- infrared wavelength regimes. C1 CALTECH, Pasadena, CA 91125 USA. Penn State Univ, University Pk, PA 16802 USA. Jet Prop Lab, NASA, Pasadena, CA 91109 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. RP Segura, A (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Circuito Exterior,CU Apartado Postal 70-543, Mexico City 04510, DF, Mexico. EM antigona@nucleares.unam.mx NR 76 TC 65 Z9 65 U1 2 U2 28 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2007 VL 472 IS 2 BP 665 EP 679 DI 10.1051/0004-6361:20066663 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214SN UT WOS:000249758500040 ER PT J AU Chifor, C Tripathi, D Mason, HE Dennis, BR AF Chifor, C. Tripathi, D. Mason, H. E. Dennis, B. R. TI Ray precursors to flares and filament eruptions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : filaments; Sun : prominences; Sun : coronal mass ejections (CMEs); Sun : flares; Sun : UV radiation; Sun : X-rays, gamma rays ID CORONAL MASS EJECTIONS; X-RAY; SOLAR-FLARES; MAGNETIC-FLUX; RADIO OBSERVATIONS; TRACE OBSERVATIONS; ATOMIC DATABASE; EMISSION-LINES; ENERGY-RELEASE; SOURCE REGIONS AB Aims. To study preflare X- ray brightenings as diagnostics of the destabilisation of flare- associated erupting filaments/ prominences. Methods. We combine new observations from the Transition Region and Coronal Explorer ( TRACE) and the Reuven Ramaty High Energy Solar Spectroscopic Imager ( RHESSI), as well as revisit events reported in the literature to date, in order to scrutinise the preflare activity during eight flare- associated filament eruptions. Results. The preflare activity occurs in the form of discrete, localised X- ray brightenings observed between 2 and 50 min before the impulsive phase of the flare and filament acceleration. These transient preflare brightenings are situated on or near ( within 10" of) the polarity inversion line ( PIL), coincident with emerging and/ or canceling magnetic flux. The filaments begin to rise from the location of the preflare brightenings. In five out of eight events, the preflare brightenings were observed beneath the filament channel, close to the filament footpoint first observed to rise. Both thermal and nonthermal hard X- ray emissions during the preflare enhancement were detected with RHESSI, suggesting that both plasma heating and electron acceleration occurred at this time. The main energy release during the impulsive phase of the flare is observed close to ( within 50" of) the preflare brightenings. The fast- rise phase of the filament eruption starts at the same time as the onset of the main flare or up to 5 min later. Conclusions. The preflare brightenings are precursors to the flare and filament eruption. These precursors represent distinct, localised instances of energy release, rather than a gradual energy release prior to the main flare. The X- ray precursors represent clearly observable signatures in the early stages of the eruption. Together with the timing of the filament fast- rise at or after the main flare onset, the X- ray precursors provide evidence for a tether- cutting mechanism initially manifested as localised magnetic reconnection being a common trigger for both flare emission and filament eruption. C1 Ctr Math Sci, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chifor, C (reprint author), Ctr Math Sci, Dept Appl Math & Theoret Phys, Wilberforce Rd, Cambridge CB3 0WA, England. EM c.chifor@damtp.cam.ac.uk; d.tripathi@damtp.cam.ac.uk; h.e.mason@damtp.cam.ac.uk; brian.r.dennis@nasa.gov RI Dennis, Brian/C-9511-2012; Tripathi, Durgesh/D-9390-2012 OI Tripathi, Durgesh/0000-0003-1689-6254 NR 75 TC 49 Z9 49 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2007 VL 472 IS 3 BP 967 EP U46 DI 10.1051/0004-6361:20077771 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214SO UT WOS:000249758600031 ER PT J AU Pottasch, SR Bernard-Salas, J Roellig, TL AF Pottasch, S. R. Bernard-Salas, J. Roellig, T. L. TI Abundances of planetary nebula M1-42 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : abundances; planetary nebulae : individual : M1-42; infrared : ISM ID SPITZER-SPACE-TELESCOPE; GALACTIC BULGE; CENTRAL STARS; LINES; EVOLUTION; SPECTRA; CATALOG; FLUXES; IC-418 AB The spectra of the planetary nebula M1-42 is reanalysed using spectral measurements made in the mid-infrared with the Spitzer Space Telescope. The aim is to determine the chemical composition of this object. We also make use of ISO, IUE and ground based spectra. Abundances determined from the mid-and far-infrared lines, which are insensitive to electron temperature, are used as the basis for the determination of the composition, which are found to substantially differ from earlier results. High values of neon, argon and sulfur are found. They are higher than in other PN, with the exception of NGC6153, a nebula of very similar abundances. The high values of helium and nitrogen found indicate that the second dredge-up and hot bottom burning has occurred in the course of evolution and that the central star was originally more massive than 4 M(circle dot). The present temperature and luminosity of the central star is determined and at first sight may be inconsistent with such a high mass. C1 Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pottasch, SR (reprint author), Univ Groningen, Kapteyn Astron Inst, PO Box 800, NL-9700 AV Groningen, Netherlands. EM pottasch@astro.rug.nl NR 40 TC 6 Z9 6 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2007 VL 471 IS 3 BP 865 EP 872 DI 10.1051/0004-6361:20077381 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199FY UT WOS:000248682800019 ER PT J AU de Val-Borro, M Artymowicz, P D'Angelo, G Peplinski, A AF de Val-Borro, M. Artymowicz, P. D'Angelo, G. Peplinski, A. TI Vortex generation in protoplanetary disks with an embedded giant planet SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planet and satellites : general; accretion, accretion disks; hydrodynamics; instabilities; methods : numerical ID ROSSBY-WAVE INSTABILITY; DIFFERENTIALLY ROTATING-DISKS; ANGULAR-MOMENTUM TRANSPORT; THIN ACCRETION DISKS; VORTICITY GENERATION; NUMERICAL-SIMULATION; NONLINEAR STABILITY; DYNAMICAL STABILITY; HYDRODYNAMIC CODE; SHEAR INSTABILITY AB Context. Vortices in protoplanetary disks can capture solid particles and form planetary cores within shorter timescales than those involved in the standard core-accretion model. Aims. We investigate vortex generation in thin unmagnetized protoplanetary disks with an embedded giant planet with planet to star mass ratio 10(-4) and 10(-3). Methods. Two-dimensional hydrodynamical simulations of a protoplanetary disk with a planet are performed using two different numerical methods. The results of the non-linear simulations are compared with a time-resolved modal analysis of the azimuthally averaged surface density profiles using linear perturbation theory. Results. Finite-difference methods implemented in polar coordinates generate vortices moving along the gap created by Neptunemass to Jupiter-mass planets. The modal analysis shows that unstable modes are generated with growth rate of order 0.3 ohm(K) for azimuthal numbers m = 4; 5; 6, where ohm(K) is the local Keplerian frequency. Shock-capturing Cartesian-grid codes do not generate very much vorticity around a giant planet in a standard protoplanetary disk. Modal calculations confirm that the obtained radial profiles of density are less susceptible to the growth of linear modes on timescales of several hundreds of orbital periods. Navier-Stokes viscosity of the order nu = 10(-5) ( in units of a(2) ohm(p)) is found to have a stabilizing effect and prevents the formation of vortices. This result holds at high resolution runs and using different types of boundary conditions. Conclusions. Giant protoplanets of Neptune-mass to Jupiter-mass can excite the Rossby wave instability and generate vortices in thin disks. The presence of vortices in protoplanetary disks has implications for planet formation, orbital migration, and angular momentum transport in disks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stockholm Univ, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. Univ Toronto, Toronto, ON M5S 1A4, Canada. NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP de Val-Borro, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mdeval@cfa.harvard.edu RI de Val-Borro, Miguel/H-1319-2013; D'Angelo, Gennaro/L-7676-2014; OI de Val-Borro, Miguel/0000-0002-0455-9384; D'Angelo, Gennaro/0000-0002-2064-0801; Peplinski, Adam/0000-0002-7448-3290 NR 57 TC 57 Z9 57 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2007 VL 471 IS 3 BP 1043 EP 1055 DI 10.1051/0004-6361:20077169 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199FY UT WOS:000248682800037 ER PT J AU Shikaze, Y Haino, S Abe, K Fuke, H Hams, T Kim, KC Makida, Y Matsuda, S Mitchell, JW Moiseev, AA Nishimura, J Nozaki, M Orito, S Ormes, JF Sanuki, T Sasaki, M Seo, ES Streitmatter, RE Suzuki, J Tanaka, K Yamagami, T Yamamoto, A Yoshida, T Yoshimura, K AF Shikaze, Y. Haino, S. Abe, K. Fuke, H. Hams, T. Kim, K. C. Makida, Y. Matsuda, S. Mitchell, J. W. Moiseev, A. A. Nishimura, J. Nozaki, M. Orito, S. Ormes, J. F. Sanuki, T. Sasaki, M. Seo, E. S. Streitmatter, R. E. Suzuki, J. Tanaka, K. Yamagami, T. Yamamoto, A. Yoshida, T. Yoshimura, K. TI Measurements of 0.2-20 GeV/n cosmic-ray proton and helium spectra from 1997 through 2002 with the BESS spectrometer SO ASTROPARTICLE PHYSICS LA English DT Article DE cosmic-ray proton; cosmic-ray helium; atmospheric proton; solar modulation; superconducting spectrometer ID SMALL ATMOSPHERIC DEPTHS; ANTIPROTON SPECTRUM; ONBOARD BESS; PROGRESS AB We measured low energy cosmic-ray proton and helium spectra in the kinetic energy range 0.215-21.5 GeV/n at different solar activities during a period from 1997 to 2002. The observations were carried out with the BESS spectrometer launched on a balloon at Lynn Lake, Canada. A calculation for the correction of secondary particle backgrounds from the overlying atmosphere was improved by using the measured spectra at small atmospheric depths ranging from 5 through 37 g/cm(2). The uncertainties including statistical and systematic errors of the obtained spectra at the top of atmosphere are 5-7% for protons and 6-9% for helium nuclei in the energy range 0.5-5 GeV/n. (C) 2007 Elsevier B.V. All rights reserved. C1 KEK, Tsukuba, Ibaraki 3050801, Japan. Kobe Univ, Kobe, Hyogo 6578501, Japan. Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Kanagawa 2298510, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. Univ Tokyo, Bunkyo Ku, Tokyo 1130033, Japan. RP Haino, S (reprint author), KEK, Tsukuba, Ibaraki 3050801, Japan. EM haino@post.kek.jp OI Seo, Eun-Suk/0000-0001-8682-805X NR 35 TC 110 Z9 111 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD SEP PY 2007 VL 28 IS 1 BP 154 EP 167 DI 10.1016/j.astropartphys.2007.05.001 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 223FO UT WOS:000250355200014 ER PT J AU Murphy, KD Yaqoob, T Terashima, Y AF Murphy, Kendrah D. Yaqoob, Tahir Terashima, Yuichi TI Monitoring the violent activity from the inner accretion disk of the Seyfert 1.9 galaxy NGC 2992 with RXTE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : Seyfert; line : profiles; X-rays : individual ( NGC 2992) ID X-RAY VARIABILITY; FEK-ALPHA; NGC 2992; SPECTRUM; TORUS; LINES; AGN AB We present the results of a 1 year monitoring campaign of the Seyfert 1.9 galaxy NGC 2992 with RXTE. Historically, the source has been shown to vary dramatically in 2-10 keV flux over timescales of years and was thought to be slowly transitioning between periods of quiescence and active accretion. Our results show that in 1 year the source continuum flux covered almost the entire historical range, making it unlikely that the low-luminosity states correspond to the accretion mechanism switching off. During flaring episodes we found that a highly redshifted Fe K line appears, implying that the violent activity is occurring in the inner accretion disk, within similar to 100 gravitational radii of the central black hole. We also found that the spectral index of the X-ray continuum remained approximately constant during the large amplitude variability. These observations make NGC 2992 well-suited for future multiwaveband monitoring, as a test bed for constraining accretion models. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Div Sci, Greenbelt, MD 20771 USA. Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. RP Murphy, KD (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NR 29 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2007 VL 666 IS 1 BP 96 EP 108 DI 10.1086/520039 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QH UT WOS:000249058600009 ER PT J AU Beckmann, V Gehrels, N Tueller, J AF Beckmann, V. Gehrels, N. Tueller, J. TI The 1-200 keV X-ray spectrum of NGC 2992 and NGC 3081 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual ( NGC 2992, NGC 3081); galaxies : Seyfert; X-rays : galaxies ID EMISSION-LINE GALAXIES; ACCRETION DISKS; NGC 2992; AGN; VARIABILITY; MISSION; CATALOG AB The Seyfert 2 galaxies NGC 2992 and NGC 3081 have been observed by INTEGRAL and Swift. We report the results and a comparison of the spectrum above 10 keV based on INTEGRAL IBIS/ISGRI, Swift/BAT, and BeppoSAX/PDS. A spectrum can be extracted in the X-ray energy band ranging from 1 up to 200 keV. Although NGC 2992 shows a complex spectrum below 10 keV, the hard tail observed by various missions exhibits a slope of Gamma = 2, independent of the flux level during the observation. No cut-off is detectable up to the detection limit around 200 keV. In addition, NGC 3081 is detected in the INTEGRAL and Swift observation and also shows an unbroken Gamma = 1: 8 spectrum upto 150 keV. These two Seyfert galaxies give further evidence that a high-energy cut-off in the hard X-ray spectra is often located at energies E-C >> 100 keV. In NGC 2992 a constant spectral shape is observed over a hard X-ray luminosity variation by a factor of 11. This might indicate that the physical conditions of the emitting hot plasma are constant, while the amount of plasma varies, due to long-term flaring activity. C1 NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Ctr Astrophys Sci, Greenbelt, MD 20771 USA. Univ Maryland, Dept Phys, Baltimore, MD 21201 USA. INTEGRAL, Sci Data Ctr, CH-1290 Versoix, Switzerland. RP Beckmann, V (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Code 661, Greenbelt, MD 20771 USA. RI Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012 NR 24 TC 11 Z9 11 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2007 VL 666 IS 1 BP 122 EP 127 DI 10.1086/519486 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QH UT WOS:000249058600011 ER PT J AU Temi, P Brighenti, F Mathews, WG AF Temi, Pasquale Brighenti, Fabrizio Mathews, William G. TI Spitzer observations of transient, extended dust in two elliptical galaxies: New evidence of recent feedback energy release in galactic cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : ISM; infrared : galaxies; infrared : ISM ID SUPERMASSIVE BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; IONIZED-GAS; X-RAY; CHANDRA OBSERVATIONS; INTERSTELLAR GRAINS; INFRARED-EMISSION; COOLING FLOWS; HOT GAS; STELLAR AB Spitzer observations of extended dust in two optically normal elliptical galaxies provide a new confirmation of buoyant feedback outflow in the hot gas atmospheres around these galaxies. AGN feedback energy is required to prevent wholesale cooling and star formation in these group-centered galaxies. In NGC 5044 we observe interstellar (presumably PAH) emission at 8 mu m out to about 5 kpc. Both NGC 5044 and NGC 4636 have extended 70 mu m emission from cold dust exceeding that expected from stellar mass loss. The sputtering lifetime of this extended dust in the similar to 1 keV interstellar gas, similar to 10(7) yr, establishes the time when the dust first entered the hot gas. Evidently the extended dust originated in dusty disks or clouds, commonly observed in elliptical galaxy cores, that were disrupted, heated, and buoyantly transported outward. The surviving central dust in NGC 5044 and NGC 4636 has been disrupted into many small filaments. It is remarkable that the asymmetrically extended 8 mu m emission in NGC 5044 is spatially coincident with H alpha+[N II] emission from warm gas. A calculation shows that dust-assisted cooling in buoyant hot gas moving out from the galactic core can cool within a few kiloparsecs in similar to 10(7) yr, explaining the optical line emission observed. The X-ray images of both galaxies are disturbed. All timescales for transient activity - restoration of equilibrium and buoyant transport in the hot gas, dynamics of surviving dust fragments, and dust sputtering - are consistent with a central release of feedback energy in both galaxies about 107 years ago. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. Univ Calif Santa Cruz, Board Studies Astron & Astrophys, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. RP Temi, P (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM ptemi@mail.arc.nasa.gov; fabrizio.brighenti@unibo.it; mathews@ucolick.org NR 38 TC 35 Z9 36 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2007 VL 666 IS 1 BP 222 EP 230 DI 10.1086/520123 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QH UT WOS:000249058600021 ER PT J AU Abdo, AA Allen, BT Berley, D Blaufuss, E Casanova, S Dingus, BL Ellsworth, RW Gonzalez, MM Goodman, JA Hays, E Hoffman, CM Kolterman, BE Lansdell, CP Linnemann, JT McEnery, JE Mincer, AI Nemethy, P Noyes, D Ryan, JM Samuelson, FW Parkinson, PMS Shoup, A Sinnis, G Smith, AJ Sullivan, GW Vasileiou, V Walker, GP Williams, DA Xu, XW Yodh, GB AF Abdo, A. A. Allen, B. T. Berley, D. Blaufuss, E. Casanova, S. Dingus, B. L. Ellsworth, R. W. Gonzalez, M. M. Goodman, J. A. Hays, E. Hoffman, C. M. Kolterman, B. E. Lansdell, C. P. Linnemann, J. T. McEnery, J. E. Mincer, A. I. Nemethy, P. Noyes, D. Ryan, J. M. Samuelson, F. W. Parkinson, P. M. Saz Shoup, A. Sinnis, G. Smith, A. J. Sullivan, G. W. Vasileiou, V. Walker, G. P. Williams, D. A. Xu, X. W. Yodh, G. B. TI Milagro constraints on very high energy emission from short-duration gamma-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; gamma rays : observations ID GRB 970417A; HOST GALAXY; TEV; AFTERGLOW; DISCOVERY; GRB-050709; TELESCOPE; SEARCH; FLARES; ARRAY AB Recent rapid localizations of short, hard gamma-ray bursts (GRBs) by the Swift and HETE satellites have led to the observation of the first afterglows and the measurement of the first redshifts from this type of burst ( Fox et al. 2005; Gehrels et al. 2005; Villasenor et al. 2005; Berger et al. 2005; Barthelmy et al. 2005). Detection of > 100 GeV counterparts would place powerful constraints on GRB mechanisms. Seventeen short-duration (< 5 s) GRBs detected by satellites occurred within the field of view of the Milagro gamma-ray observatory between 2000 January and 2006 December. We have searched the Milagro data for > 100 GeV counterparts to these GRBs and find no significant emission correlated with these bursts. Due to the absorption of high-energy gamma rays by the extragalactic background light (EBL), detections are only expected for redshifts less than similar to 0.5. While most long-duration GRBs occur at redshifts higher than 0.5, the opposite is thought to be true of short GRBs. Lack of a detected VHE signal thus allows setting meaningful fluence limits. One GRB in the sample (050509b) has a likely association with a galaxy at a redshift of 0.225, while another ( 051103) has been tentatively linked to the nearby galaxy M81. Fluence limits are corrected for EBL absorption, either using the known measured redshift, or computing the corresponding absorption for a redshift of 0.1 and 0.5, as well as for the case of z = 0. C1 Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Los Alamos Natl Lab, Dept Phys, Los Alamos, NM 87545 USA. George Mason Univ, Dept Phys, Fairfax, VA 22030 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. NYU, Dept Phys, New York, NY 10003 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. US FDA, Ctr Devices & Radiol Hlth, Office Sci & Engn Lab, Rockville, MD 20857 USA. Univ Calif Santa Cruz, Inst Particle Phys, Santa Cruz, CA 95064 USA. Ohio State Univ, Lima, OH 45804 USA. Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Abdo, AA (reprint author), Argonne Natl Lab, Div High Energy Phys, 9700 S Cass Ave, Argonne, IL 60439 USA. RI McEnery, Julie/D-6612-2012; Hays, Elizabeth/D-3257-2012; Casanova, Sabrina/J-8935-2013; OI Casanova, Sabrina/0000-0002-6144-9122; Dingus, Brenda/0000-0001-8451-7450; Mincer, Allen/0000-0002-6307-1418 NR 51 TC 29 Z9 29 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2007 VL 666 IS 1 BP 361 EP 367 DI 10.1086/519763 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QH UT WOS:000249058600034 ER PT J AU Haghighipour, N Raymond, SN AF Haghighipour, Nader Raymond, Sean N. TI Habitable planet formation in binary planetary systems SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; celestial mechanics; planetary systems; planets and satellites : formation; solar system : formation ID HIGH-RESOLUTION SIMULATIONS; CARBON-DIOXIDE CLOUDS; EARTH-LIKE PLANETS; TERRESTRIAL PLANETS; STAR SYSTEMS; DYNAMICAL STABILITY; WATER DELIVERY; GIANT PLANETS; ACCRETION; DISK AB Recent radial velocity observations have indicated that Jovian-type planets can exist in moderately close binary star systems. Numerical simulations of the dynamical stability of terrestrial-class planets in such environments have shown that, in addition to their giant planets, these systems can also harbor Earth-like objects. In this paper we study the late stage of terrestrial planet formation in such binary planetary systems, and present the results of the simulations of the formation of Earth-like bodies in their habitable zones. We consider a circumprimary disk of Moon-to Marssized objects and numerically integrate the orbits of these bodies at the presence of the Jovian-type planet of the system and for different values of the mass, semimajor axis, and orbital eccentricity of the secondary star. Results indicate that Earth-like objects, with substantial amounts of water, can form in the habitable zone of the primary star. Simulations also indicate that by transferring angular momentum from the secondary star to protoplanetary objects, the giant planet of the system plays a key role in the radial mixing of these bodies and the water contents of the final terrestrial planets. We will discuss the results of our simulation and show that the formation of habitable planets in binary planetary systems is more probable in binaries with moderate to large perihelia. C1 Univ Hawaii Manoa, Inst Astrobiol, Honolulu, HI 96822 USA. NASA, Inst Astron, Honolulu, HI 96822 USA. Univ Colorado, Ctr Astrobiol, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. RP Haghighipour, N (reprint author), Univ Hawaii Manoa, Inst Astrobiol, Honolulu, HI 96822 USA. EM nader@ifa.hawaii.edu; raymond@lasp.colorado.edu NR 51 TC 39 Z9 39 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2007 VL 666 IS 1 BP 436 EP 446 DI 10.1086/520501 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QH UT WOS:000249058600041 ER PT J AU Chen, CH Li, A Bohac, C Kim, KH Watson, DM van Cleve, J Houck, J Stapelfeldt, K Werner, MW Rieke, G Su, K Marengo, M Backman, D Beichman, C Fazio, G AF Chen, C. H. Li, A. Bohac, C. Kim, K. H. Watson, D. M. van Cleve, J. Houck, J. Stapelfeldt, K. Werner, M. W. Rieke, G. Su, K. Marengo, M. Backman, D. Beichman, C. Fazio, G. TI The dust and gas around beta Pictoris SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : formation; planetary systems : protoplanetary disks; stars : individual (beta Pictoris) ID SPITZER-SPACE-TELESCOPE; INTERSTELLAR SILICATE MINERALOGY; PHOTON-STIMULATED DESORPTION; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISK; PLANETARY-SYSTEMS; ATOMIC DATA; CORONAGRAPHIC OBSERVATIONS; INFRARED SPECTROGRAPH; IMAGING POLARIMETRY AB We have obtained Spitzer IRS 5.5-35 mu m spectroscopy of the debris disk around beta Pictoris. In addition to the 10 mu m silicate emission feature originally observed from the ground, we also detect the crystalline silicate emission bands at 28 and 33.5 mu m. This is the first time that the silicate bands at wavelengths longer than 10 mu m have ever been seen in the beta Pictoris disk. The observed dust emission is well reproduced by a dust model consisting of fluffy cometary and crystalline olivine aggregates. We searched for line emission from molecular hydrogen and atomic [S I], Fe II, and Si II gas but detected none. We place a 3 sigma upper limit of < 17M(circle plus) on the H-2 S(1) gas mass, assuming an excitation temperature of T-ex 100 K. This suggests that there is less gas in this system than is required to form the envelope of Jupiter. We hypothesize that some of the atomic Na I gas observed in Keplerian rotation around beta Pictoris may be produced by photon-stimulated desorption from circumstellar dust grains. C1 Natl Opt Astron Observ, Tucson, AZ 85726 USA. Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Chen, CH (reprint author), Natl Opt Astron Observ, Tucson, AZ 85726 USA. EM cchen@noao.edu; lia@missouri.edu RI Stapelfeldt, Karl/D-2721-2012 NR 77 TC 46 Z9 46 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2007 VL 666 IS 1 BP 466 EP 474 DI 10.1086/519989 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QH UT WOS:000249058600043 ER PT J AU Fortney, JJ Marley, MS AF Fortney, Jonathan J. Marley, Mark S. TI Analysis of SPITZER spectra of irradiated planets: Evidence for water vapor? SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; radiative transfer; stars : individual (HD 189733, HD 209458) ID EXTRASOLAR GIANT PLANETS; HD 189733B; THERMAL STRUCTURE; HOT JUPITERS; LIGHT CURVES; T-DWARFS; ATMOSPHERES; PHOTOMETRY; CHEMISTRY; EMISSION AB Published mid-infrared spectra of transiting planets HD 209458b and HD 189733b, obtained during secondary eclipse by the InfraRed Spectrograph (IRS) aboard the Spitzer Space Telescope, are predominantly featureless. In particular, these flux ratio spectra do not exhibit an expected feature arising from water vapor absorption shortward of. Here we suggest that in the absence of flux variability, the spectral data for HD 189733b 10 mu m are inconsistent with 8 mu m photometry obtained with Spitzer's InfraRed Array Camera (IRAC), perhaps an indication of problems with the challenging reduction of the IRS spectra. The IRAC point, along with previously published secondary eclipse photometry for HD 189733b, are in good agreement with a one-dimensional model of HD 189733b that clearly shows absorption due to water vapor in the emergent spectrum. We are not able to draw firm conclusions regarding the IRS data for HD 209458b, but spectra predicted by 1D and 3D atmosphere models fit the data adequately, without adjustment of the water abundance or reliance on cloud opacity. We argue that the generally good agreement between model spectra and IRS spectra of brown dwarfs with atmospheric temperatures similar to these highly irradiated planets lends confidence in the modeling procedure. C1 NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. RP Fortney, JJ (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. EM jfortney@arc.nasa.gov; mark.s.marley@nasa.gov RI Marley, Mark/I-4704-2013; OI Fortney, Jonathan/0000-0002-9843-4354 NR 40 TC 34 Z9 34 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2007 VL 666 IS 1 BP L45 EP L48 DI 10.1086/521603 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QJ UT WOS:000249058800012 ER PT J AU Kashlinsky, A Arendt, RG Mather, J Moseley, SH AF Kashlinsky, A. Arendt, R. G. Mather, J. Moseley, S. H. TI Demonstrating the negligible contribution of optical HST ACS galaxies to source-subtracted cosmic infrared background fluctuations in deep Spitzer Irac images SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; diffuse radiation; early universe ID ANISOTROPIES; SPECTRUM; STARS; MAPS AB We study the possible contribution of optical galaxies detected with the Hubble ACS instrument to the near-IR cosmic infrared (CIB) fluctuations in deep Spitzer images. The Spitzer data used in this analysis are obtained in the course of the GOODS project, from which we select four independent 10' x 10' regions observed at both 3.6 and 4.5 mu m. ACS source catalogs for all of these areas are used to construct maps containing only their emissions in the ACS bands. We find that deep Spitzer data exhibit CIB fluctuations remaining after removal B, V, i, z of foreground galaxies of a very different clustering pattern at both 3.6 and 4.5 mm than the ACS galaxies could contribute. We also find that there are very good correlations between the ACS galaxies and the removed galaxies in the Spitzer maps, but practically no correlations remain with the residual Spitzer maps used to identify the CIB fluctuations. These contributions become negligible on larger scales used to probe the CIB fluctuations arising from clustering. This means that the ACS galaxies cannot contribute to the large-scale CIB fluctuations found in the residual Spitzer data. The absence of their contributions also means that the CIB fluctuations arise at as the Lyman break of their sources must be redshifted past the longest ACS band, or the fluctuations z greater than or similar to 6.5 have to originate in the more local but extremely low luminosity galaxies. C1 NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Kashlinsky, A (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM kashlinsky@milkyway.gsfc.nasa.gov; arendt@milkyway.gsfc.nasa.gov; mather@milkyway.gsfc.nasa.gov; moseley@milkyway.gsfc.nasa.gov RI Moseley, Harvey/D-5069-2012; OI Arendt, Richard/0000-0001-8403-8548 NR 22 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 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2007 VL 666 IS 1 BP L1 EP L4 DI 10.1086/521551 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204QJ UT WOS:000249058800001 ER PT J AU Scoville, N Abraham, RG Aussel, H Barnes, JE Benson, A Blain, AW Calzetti, D Comastri, A Capak, P Carilli, C Carlstrom, JE Carollo, CM Colbert, J Daddi, E Ellis, RS Elvis, M Ewald, SP Fall, M Franceschini, A Giavalisco, M Green, W Griffiths, RE Guzzo, L Hasinger, G Impey, C Kneib, JP Koda, J Koekemoer, A Lefevre, O Lilly, S Liu, CT McCracken, HJ Massey, R Mellier, Y Miyazaki, S Mobasher, B Mould, J Norman, C Refregier, A Renzini, A Rhodes, J Rich, M Sanders, DB Schiminovich, D Schinnerer, E Scodeggio, M Sheth, K Shopbell, PL Taniguchi, Y Tyson, ND Urry, CM Van Waerbeke, L Vettolani, P White, SDM Yan, L AF Scoville, N. Abraham, R. G. Aussel, H. Barnes, J. E. Benson, A. Blain, A. W. Calzetti, D. Comastri, A. Capak, P. Carilli, C. Carlstrom, J. E. Carollo, C. M. Colbert, J. Daddi, E. Ellis, R. S. Elvis, M. Ewald, S. P. Fall, M. Franceschini, A. Giavalisco, M. Green, W. Griffiths, R. E. Guzzo, L. Hasinger, G. Impey, C. Kneib, J.-P. Koda, J. Koekemoer, A. Lefevre, O. Lilly, S. Liu, C. T. McCracken, H. J. Massey, R. Mellier, Y. Miyazaki, S. Mobasher, B. Mould, J. Norman, C. Refregier, A. Renzini, A. Rhodes, J. Rich, M. Sanders, D. B. Schiminovich, D. Schinnerer, E. Scodeggio, M. Sheth, K. Shopbell, P. L. Taniguchi, Y. Tyson, N. D. Urry, C. M. Van Waerbeke, L. Vettolani, P. White, S. D. M. Yan, L. TI COSMOS: Hubble space telescope observations SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; dark matter; galaxies : evolution; galaxies : formation; large-scale structure of universe; surveys ID DEEP FIELD AB The Cosmic Evolution Survey ( COSMOS) was initiated with an extensive allocation ( 590 orbits in Cycles 12 - 13) using the Hubble Space Telescope ( HST) for high-resolution imaging. Here we review the characteristics of the HST imaging with the Advanced Camera for Surveys ( ACS) and parallel observations with NICMOS and WFPC2. A square field ( 1.8 deg(2)) has been imaged with single-orbit ACS I-band F814W exposures with 50% completeness for sources 0.5 '' in diameter at I-AB= 26. 0 mag. The ACS is a key part of the COSMOS survey, providing very high sensitivity and high-resolution ( 0.09 '' FWHM and 0.05 '' pixels) imaging and detecting a million objects. These images yield resolved morphologies for several hundred thousand galaxies. The small HST PSF also provides greatly enhanced sensitivity for weak-lensing investigations of the dark matter distribution. C1 CALTECH, Pasadena, CA 91125 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Chicago, Dept Phys, Chicago, IL 60637 USA. ETH, Dept Phys, CH-8093 Zurich, Switzerland. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Osserv Astron Brera, I-20121 Milan, Italy. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Astrophys Lab, F-13376 Marseille 12, France. CUNY Coll Staten Isl, Astron Observ, Staten Isl, NY 10314 USA. Univ Paris 06, CNRS, UMR7095, Inst Astrophys, F-75014 Paris, France. Observ Paris, LERMA, F-75014 Paris, France. Natl Astron Observ, Subaru Telescope, Hilo, HI 96720 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. European So Observ, D-85748 Garching, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. CNR, Inst Astrophys Spatiale & Fis Cosm, I-20133 Milan, Italy. Ehime Univ, Sch Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. Amer Museum Nat Hist, New York, NY 10024 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Inst Astrophys, F-75014 Paris, France. Max Planck Inst Astrophys, D-85748 Garching, Germany. RP Scoville, N (reprint author), CALTECH, MC 105-24,1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Le Fevre, Olivier/G-7389-2011; Daddi, Emanuele/D-1649-2012; Urry, Claudia/G-7381-2011; Kneib, Jean-Paul/A-7919-2015; Comastri, Andrea/O-9543-2015; OI Daddi, Emanuele/0000-0002-3331-9590; Urry, Claudia/0000-0002-0745-9792; Kneib, Jean-Paul/0000-0002-4616-4989; Comastri, Andrea/0000-0003-3451-9970; Scodeggio, Marco/0000-0002-2282-5850; Koekemoer, Anton/0000-0002-6610-2048; Schinnerer, Eva/0000-0002-3933-7677 NR 26 TC 242 Z9 243 U1 1 U2 12 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 38 EP 45 DI 10.1086/516580 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000004 ER PT J AU Capak, P Aussel, H Ajiki, M McCracken, HJ Mobasher, B Scoville, N Shopbell, P Taniguchi, Y Thompson, D Tribiano, S Sasaki, S Blain, AW Brusa, M Carilli, C Comastri, A Carollo, CM Cassata, P Colbert, J Ellis, RS Elvis, M Giavalisco, M Green, W Guzzo, L Hasinger, G Ilbert, O Impey, C Jahnke, K Kartaltepe, J Kneib, JP Koda, J Koekemoer, A Komiyama, Y Leauthaud, A Lefevre, O Lilly, S Liu, C Massey, R Miyazaki, S Murayama, T Nagao, T Peacock, JA Pickles, A Porciani, C Renzini, A Rhodes, J Rich, M Salvato, M Sanders, DB Scarlata, C Schiminovich, D Schinnerer, E Scodeggio, M Sheth, K Shioya, Y Tasca, LAM Taylor, JE Yan, L Zamorani, G AF Capak, P. Aussel, H. Ajiki, M. McCracken, H. J. Mobasher, B. Scoville, N. Shopbell, P. Taniguchi, Y. Thompson, D. Tribiano, S. Sasaki, S. Blain, A. W. Brusa, M. Carilli, C. Comastri, A. Carollo, C. M. Cassata, P. Colbert, J. Ellis, R. S. Elvis, M. Giavalisco, M. Green, W. Guzzo, L. Hasinger, G. Ilbert, O. Impey, C. Jahnke, K. Kartaltepe, J. Kneib, J.-P. Koda, J. Koekemoer, A. Komiyama, Y. Leauthaud, A. Lefevre, O. Lilly, S. Liu, C. Massey, R. Miyazaki, S. Murayama, T. Nagao, T. Peacock, J. A. Pickles, A. Porciani, C. Renzini, A. Rhodes, J. Rich, M. Salvato, M. Sanders, D. B. Scarlata, C. Schiminovich, D. Schinnerer, E. Scodeggio, M. Sheth, K. Shioya, Y. Tasca, L. A. M. Taylor, J. E. Yan, L. Zamorani, G. TI The first release COSMOS optical and near-IR data and catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; galaxies : evolution; large-scale structure of universe; surveys ID HUBBLE-DEEP-FIELD; LYMAN-BREAK GALAXIES; ULTRAVIOLET LUMINOSITY DENSITY; FRANCE-HAWAII-TELESCOPE; EVOLUTION SURVEY COSMOS; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; WIDE-FIELD; PHOTOMETRIC REDSHIFTS; IMAGING SURVEY AB We present imaging data and photometry for the COSMOS survey in 15 photometric bands between 0.3 and 2.4 mu m. These include data taken on the Subaru 8.3 m telescope, the KPNO and CTIO 4 m telescopes, and the CFHT 3.6 m telescope. Special techniques are used to ensure that the relative photometric calibration is better than 1% across the field of view. The absolute photometric accuracy from standard-star measurements is found to be 6%. The absolute calibration is corrected using galaxy spectra, providing colors accurate to 2% or better. Stellar and galaxy colors and counts agree well with the expected values. Finally, as the first step in the scientific analysis of these data we construct panchromatic number counts which confirm that both the geometry of the universe and the galaxy population are evolving. C1 CALTECH, Pasadena, CA 91125 USA. Univ Paris 07, CNRS, UMR 7158, AIM,Unite Mixte Rech, F-91191 Gif Sur Yvette, France. Tohoku Univ, Grad Sch Sci, Inst Astron, Sendai, Miyagi 9808578, Japan. Univ Paris 06, CNRS, Inst Astrophys, UMR 7095, F-75014 Paris, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Ehime Univ, Grad Sch Sci & Engn, Dept Phys, Matsuyama, Ehime 7908577, Japan. Univ Arizona, LBT Observ, Tucson, AZ 85721 USA. Amer Museum Nat Hist, New York, NY 10024 USA. CUNY, Borough Manhattan Community Coll, New York, NY 10007 USA. Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. Natl Radio Astron Observ, Socorro, NM 87801 USA. Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. ETH, Dept Phys, CH-8093 Zurich, Switzerland. Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Astrophys Lab, F-13376 Marseille 12, France. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Natl Astron Observ, Subaru Telescope, Hilo, HI 96720 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. CALTECH, Opt Observ, Pasadena, CA 91125 USA. European So Observ, D-85748 Garching, Germany. Univ Padua, Dipartmento Astron, I-35122 Padua, Italy. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. IASF, INAF, I-20133 Milan, Italy. Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. RP Capak, P (reprint author), CALTECH, MC 105-24,1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Le Fevre, Olivier/G-7389-2011; Kneib, Jean-Paul/A-7919-2015; Comastri, Andrea/O-9543-2015; OI Schinnerer, Eva/0000-0002-3933-7677; Kneib, Jean-Paul/0000-0002-4616-4989; Comastri, Andrea/0000-0003-3451-9970; Scodeggio, Marco/0000-0002-2282-5850; Jahnke, Knud/0000-0003-3804-2137; Zamorani, Giovanni/0000-0002-2318-301X; Koekemoer, Anton/0000-0002-6610-2048; Brusa, Marcella/0000-0002-5059-6848 NR 53 TC 438 Z9 440 U1 2 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 99 EP 116 DI 10.1086/519081 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000008 ER PT J AU Scoville, N Aussel, H Benson, A Blain, A Calzetti, D Capak, P Ellis, RS El-Zant, A Finoguenov, A Giavalisco, M Guzzo, L Hasinger, G Koda, J Le Fevre, O Massey, R McCracken, HJ Mobasher, B Renzini, A Rhodes, J Salvato, M Sanders, DB Sasaki, SS Schinnerer, E Sheth, K Shopbell, PL Taniguchi, Y Taylor, JE Thompson, DJ AF Scoville, N. Aussel, H. Benson, A. Blain, A. Calzetti, D. Capak, P. Ellis, R. S. El-Zant, A. Finoguenov, A. Giavalisco, M. Guzzo, L. Hasinger, G. Koda, J. Le Fevre, O. Massey, R. McCracken, H. J. Mobasher, B. Renzini, A. Rhodes, J. Salvato, M. Sanders, D. B. Sasaki, S. S. Schinnerer, E. Sheth, K. Shopbell, P. L. Taniguchi, Y. Taylor, J. E. Thompson, D. J. TI Large structures and galaxy evolution in COSMOS at z < 1.1 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; dark matter; large-scale structure of universe; surveys ID MORPHOLOGY-DENSITY RELATION; STAR-FORMING GALAXIES; RICH CLUSTER SURVEY; DARK-MATTER HALOES; VLT DEEP SURVEY; REDSHIFT SURVEY; MASS FUNCTION; STELLAR MASS; RED-SEQUENCE; Z-SIMILAR-TO-1 AB We present the first identification of large-scale structures ( LSSs) at z < 1: 1 in the Cosmic Evolution Survey ( COSMOS). The structures are identified from adaptive smoothing of galaxy counts in the pseudo-3D space ( alpha, delta, z) using the COSMOS photometric redshift catalog. The technique is tested on a simulation including galaxies distributed in model clusters and a field galaxy population-recovering structures on all scales from 10 to 200 without a priori assumptions for the structure size or density profile. The COSMOS photometric redshift catalog yields a sample of 1.5x 10(5) galaxies with redshift accuracy, Delta z(FWHM)/( 1+z) <= 0.1 at z < 1.1 down to I-AB <= 25 mag. Using this sample of galaxies, we identify 42 LSSs and clusters. Projected surface-density maps for the structures indicate multiple peaks and internal structure in many of the most massive LSSs. The stellar masses ( determined from the galactic SEDs) for the LSSs range from M-* similar to 10(11) up to similar to 3 x 10(13) M-circle dot. Five LSSs have total stellar masses exceeding 10(13)M(circle dot). ( Total masses including nonstellar baryons and dark matter are expected to be similar to 50-100 times greater.) The derived mass function for the LSSs is consistent ( within the expected Poisson and cosmic variances) with those derived from optical and X-ray studies at lower redshift. To characterize structure evolution and for comparison with simulations, we compute a new statistic: the area filling factor as a function of the overdensity value compared to the mean at surface overdensity ( f(A) [Sigma/(Sigma) over bar( z)])). The observationally determined fA has less than 1% of the surface area ( in each redshift slice) with overdensities exceeding 10: 1, and evolution to higher overdensities is seen at later epochs ( lower z); both characteristics are in good agreement with what we find using similar processing on the Millennium Simulation. Although similar variations in the filling factors as a function of overdensity and redshift are seen in the observations and simulations, we do find that the observed distributions reach higher overdensities than the simulation, perhaps indicating overmerging in the simulation. All of the LSSs show a dramatic preference for earlier SED type galaxies in the denser regions of the structures, independent of redshift. The SED types in the central 1 and 1-5 Mpc regions of each structure average about one SED type earlier than the mean type at the same redshift, corresponding to a stellar population age difference of similar to 2-4 Gyr at z =0.3 - 1. We also investigate the evolution of key galactic properties mass, luminosity, SED, and star formation rate ( SFR) - with redshift and environmental density as derived from overdensities in the full pseudo-3D cube. Both the maturity of the stellar populations and the "downsizing'' of star formation in galaxies vary strongly with redshift ( epoch) and environment. For a very broad mass range ( 10(10)-10(12) M (circle dot)), we find that galaxies in dense environments tend to be older; this is not just restricted to the most massive galaxies. C1 CALTECH, Pasadena, CA 91125 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Toronto, Canadian Inst Theoret Astrophys, McLennan Phys Labs, Toronto, ON M5S 3H8, Canada. Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. Ossrtvatorio Astron Brera, INAF, I-23807 Merate, LC, Italy. Astrophys Lab, F-13376 Marseille 12, France. Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. Observ Paris, LERMA, F-75014 Paris, France. European So Observ, D-85748 Garching, Germany. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Tohoku Univ, Grad Sch Sci, Inst Astron, Sendai, Miyagi 9808578, Japan. Ehime Univ, Grad Sch Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. Max Planck Inst Astron, D-69117 Heidelberg, Germany. CALTECH, Opt Observ, Pasadena, CA 91125 USA. Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. RP Scoville, N (reprint author), CALTECH, MC 105-24,1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Le Fevre, Olivier/G-7389-2011 OI Schinnerer, Eva/0000-0002-3933-7677; NR 72 TC 118 Z9 118 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 150 EP 181 DI 10.1086/516751 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000011 ER PT J AU Koekemoer, AM Aussel, H Calzetti, D Capak, P Giavalisco, M Kneib, JP Leauthaud, A Le Fevre, O McCracken, HJ Massey, R Mobasher, B Rhodes, J Scoville, N Shopbell, PL AF Koekemoer, A. M. Aussel, H. Calzetti, D. Capak, P. Giavalisco, M. Kneib, J.-P. Leauthaud, A. Le Fevre, O. McCracken, H. J. Massey, R. Mobasher, B. Rhodes, J. Scoville, N. Shopbell, P. L. TI The COSMOS survey: Hubble Space Telescope advanced camera for surveys observations and data processing SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; dark matter; galaxies : evolution; galaxies : formation; large-scale structure of universe; surveys ID DEEP FIELD AB We describe the details of the Hubble Space Telescope ( HST) Advanced Camera for Surveys ( ACS) Wide Field Channel ( WFC) observations of the COSMOS field, including the data calibration and processing procedures. We obtained a total of 583 orbits of HSTACS/WFC imaging in the F814W filter, covering a field that is 1.64 deg(2) in area, the largest contiguous field ever imaged with HST. The median exposure depth across the field is 2028 s ( one HSTorbit), achieving a limiting point-source depth AB( F814W) 27: 2 ( 5 sigma). We also present details of the astrometric image registration and distortion removal and image combination using MultiDrizzle, motivating the choice of our final pixel scale ( 30 mas pixel(-1)), based on the requirements for weak-lensing science. The final set of images are publicly available through the archive sites at IPAC and STScI, along with further documentation on how they were produced. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. CALTECH, Pasadena, CA 91125 USA. Astrophys Lab, F-13376 Marseille 12, France. Univ Paris 06, CNRS, Inst Astrophys, UMR7095, F-75014 Paris, France. Observ Paris, LERMA, F-75014 Paris, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Koekemoer, AM (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RI Kneib, Jean-Paul/A-7919-2015; Le Fevre, Olivier/G-7389-2011 OI Kneib, Jean-Paul/0000-0002-4616-4989; Koekemoer, Anton/0000-0002-6610-2048; NR 16 TC 310 Z9 310 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 196 EP 202 DI 10.1086/520086 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000013 ER PT J AU Rhodes, JD Massey, RJ Albert, J Collins, N Ellis, RS Heymans, C Gardner, JP Kneib, JP Koekemoer, A Leauthaud, A Mellier, Y Refregier, A Taylor, JE Van Waerbeke, L AF Rhodes, Jason D. Massey, Richard J. Albert, Justin Collins, Nicholas Ellis, Richard S. Heymans, Catherine Gardner, Jonathan P. Kneib, Jean-Paul Koekemoer, Anton Leauthaud, Alexie Mellier, Yannick Refregier, Alexander Taylor, James E. Van Waerbeke, Ludovic TI The stability of the point-spread function of the advanced camera for surveys on the Hubble Space Telescope and implications for weak gravitational lensing SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE instrumentation : detectors; surveys; techniques : image processing ID COSMIC SHEAR; SHAPELETS AB We examine the spatial and temporal stability of the Hubble Space Telescope's Advanced Camera for Surveys ( ACS) Wide Field Camera ( WFC) point-spread function ( PSF) using the 2 deg(2) COSMOS survey. This is important for studies of weak gravitational lensing, where the ability to deconvolve the PSF from galaxy shapes is of paramount importance. We show that stochastic aliasing of the PSF necessarily occurs during "drizzling.'' This aliasing is maximal if the output-pixel scale is equal to the input-pixel scale. This source of PSF variation can be significantly reduced by choosing a Gaussian drizzle kernel with a size of 0.8 input pixels and by reducing the output-pixel scale. We show that the PSF is temporally unstable, resulting in an overall slow periodic focus change in the COSMOS images. Using a modified version of the Tiny Tim PSF modeling software, we create grids of undistorted stars over a range of telescope focus values. We then use the approximately 10 well-measured stars in each COSMOS field to pick the best-fit focus value for each field. The Tiny Tim model stars can then be used to perform PSF corrections for weak lensing. We derive a parametric correction for the effect of charge transfer efficiency ( CTE) degradation on the shapes of objects in the COSMOS field as a function of observation date, position within the ACS WFC field, and object flux. Finally, we discuss future plans to improve the CTE correction. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Explorat Universe Div, Greenbelt, MD 20771 USA. Univ British Columbia, Vancouver, BC V6T 1Z1, Canada. Astrophys Lab, F-13376 Marseille 12, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. Observ Paris, LERMA, F-75014 Paris, France. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. RP Rhodes, JD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Koekemoer, Anton/0000-0002-6610-2048 NR 42 TC 95 Z9 95 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 203 EP 218 DI 10.1086/516592 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000014 ER PT J AU Leauthaud, A Massey, R Kneib, JP Rhodes, J Johnston, DE Capak, P Heymans, C Ellis, RS Koekemoer, AM Le Fevre, O Mellier, Y Refregier, A Robin, AC Scoville, N Tasca, L Taylor, JE Van Waerbeke, L AF Leauthaud, Alexie Massey, Richard Kneib, Jean-Paul Rhodes, Jason Johnston, David E. Capak, Peter Heymans, Catherine Ellis, Richard S. Koekemoer, Anton M. Le Fevre, Oliver Mellier, Yannick Refregier, Alexandre Robin, Annie C. Scoville, Nick Tasca, Lidia Taylor, James E. Van Waerbeke, Ludovic TI Weak gravitational lensing with COSMOS: Galaxy selection and shape measurements SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; gravitational lensing; large-scale structure of universe ID HUBBLE-SPACE-TELESCOPE; DARK ENERGY CONSTRAINTS; DIGITAL SKY SURVEY; DEEP FIELD SOUTH; PHOTOMETRIC REDSHIFTS; ADVANCED CAMERA; WIDE-FIELD; SHEAR; MASS; EVOLUTION AB With a primary goal of conducting precision weak-lensing measurements from space, the COSMOS survey has imaged the largest contiguous area observed by Hubble Space Telescope to date, using the Advanced Camera for Surveys ( ACS). This is the first paper in a series in which we describe our strategy for addressing the various technical challenges in the production of weak-lensing measurements from COSMOS data. We first construct a source catalog from 575 ACS/WFC tiles ( 1.64 deg(2)) subsampled at a pixel scale of 0.03 ''. Defects and diffraction spikes are carefully removed, leaving a total of 1.2 x 10(6) objects to a limiting magnitude of F814W=26.5. This catalog is made publicly available. Multiwavelength follow-up observations of the COSMOS field provide photometric redshifts for 73% of the source galaxies in the lensing catalog. We analyze and discuss the COSMOS redshift distribution and show broad agreement with other surveys to z similar to 1. Our next step is to measure the shapes of galaxies and correct them for the distortion induced by the time-varying ACS point-spread function and for charge transfer efficiency ( CTE) effects. Simulated images are used to derive the shear susceptibility factors that are necessary in transforming shape measurements into unbiased shear estimators. For every galaxy we derive a shape measurement error and utilize this quantity to extract the intrinsic shape noise of the galaxy sample. Interestingly, our results indicate that intrinsic shape noise varies little with size, magnitude, or redshift. Representing a number density of 66 galaxies per arcmin(2), the final COSMOS weak-lensing catalog contains 3.9x10(5) galaxies with accurate shape measurements. The properties of the COSMOS weak-lensing catalog described throughout this paper will provide key input numbers for the preparation and design of next-generation wide field space missions. C1 Lab Astrophys Marseille, F-13376 Marseille 12, France. CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Paris 06, CNRS, Inst Astrophys, UMR7095, F-75014 Paris, France. Observ Paris, LERMA, F-75014 Paris, France. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Observ Besancon, F-25010 Besancon, France. Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. RP Leauthaud, A (reprint author), Lab Astrophys Marseille, BP 8,Traverse Siphon, F-13376 Marseille 12, France. RI Le Fevre, Olivier/G-7389-2011; Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Koekemoer, Anton/0000-0002-6610-2048 NR 62 TC 185 Z9 188 U1 2 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 219 EP 238 DI 10.1086/516598 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000015 ER PT J AU Massey, R Rhodes, J Leauthaud, A Capak, P Ellis, R Koekemoer, A Refregier, A Scoville, N Taylor, JE Albert, J Berge, J Heymans, C Johnston, D Kneib, JP Mellier, Y Mobasher, B Semboloni, E Shopbell, P Tasca, L Van Waerbeke, L AF Massey, Richard Rhodes, Jason Leauthaud, Alexie Capak, Peter Ellis, Richard Koekemoer, Anton Refregier, Alexandre Scoville, Nick Taylor, James E. Albert, Justin Berge, Joel Heymans, Catherine Johnston, David Kneib, Jean-Paul Mellier, Yannick Mobasher, Bahram Semboloni, Elisabetta Shopbell, Patrick Tasca, Lidia Van Waerbeke, Ludovic TI COSMOS: Three-dimensional weak lensing and the growth of structure SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; gravitational lensing; large-scale structure of universe ID GALAXY REDSHIFT SURVEY; LARGE-SCALE STRUCTURE; POWER-SPECTRUM; DARK-MATTER; RICH CLUSTERS; SHEAR; TELESCOPE; SPACE; SHAPELETS; CONSTRAINTS AB We present a three-dimensional cosmic shear analysis of the Hubble Space Telescope COSMOS survey, the largest ever optical imaging program performed in space. We have measured the shapes of galaxies for the telltale distortions caused by weak gravitational lensing and traced the growth of that signal as a function of redshift. Using both 2D and 3D analyses, we measure cosmological parameters Omega (m), the density of matter in the universe, and sigma(8), the normalization of the matter power spectrum. The introduction of redshift information tightens the constraints by a factor of 3 and also reduces the relative sampling ( or "cosmic'') variance compared to recent surveys that may be larger but are only two-dimensional. From the 3D analysis, we find that sigma(8)( Omega (m)/ 0.3) (0.44) = 0. 866(+0.085)-(0.068) at 68% confidence limits, including both statistical and potential systematic sources of error in the total budget. Indeed, the absolute calibration of shear measurement methods is now the dominant source of uncertainty. Assuming instead a baseline cosmology to fix the geometry of the universe, we have measured the growth of structure on both linear and nonlinear physical scales. Our results thus demonstrate a proof of concept for tomographic analysis techniques that have been proposed for future weak-lensing surveys by a dedicated wide-field telescope in space. C1 CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Astrophys Lab, F-13376 Marseille, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Paris 06, CNRS, Inst Astrophys, UMR7095, F-75014 Paris, France. Observ Paris, LERMA, F-75014 Paris, France. Argelander Inst Astron, D-53121 Bonn, Germany. RP Massey, R (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM rjm@astro.caltech.edu RI Kneib, Jean-Paul/A-7919-2015 OI Koekemoer, Anton/0000-0002-6610-2048; Kneib, Jean-Paul/0000-0002-4616-4989 NR 77 TC 171 Z9 176 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 239 EP 253 DI 10.1086/516599 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000016 ER PT J AU Guzzo, L Cassata, P Finoguenov, A Massey, R Scoville, NZ Capak, P Ellis, RS Mobasher, B Taniguchi, Y Thompson, D Ajiki, M Aussel, H Bohringer, H Brusa, M Calzetti, D Comastri, A Franceschini, A Hasinger, G Kasliwal, MM Kitzbichler, MG Kneib, JP Koekemoer, A Leauthaud, A McCracken, HJ Murayama, T Nagao, T Rhodes, J Sanders, DB Sasaki, S Shioya, Y Tasca, L Taylor, JE AF Guzzo, L. Cassata, P. Finoguenov, A. Massey, R. Scoville, N. Z. Capak, P. Ellis, R. S. Mobasher, B. Taniguchi, Y. Thompson, D. Ajiki, M. Aussel, H. Boehringer, H. Brusa, M. Calzetti, D. Comastri, A. Franceschini, A. Hasinger, G. Kasliwal, M. M. Kitzbichler, M. G. Kneib, J.-P. Koekemoer, A. Leauthaud, A. McCracken, H. J. Murayama, T. Nagao, T. Rhodes, J. Sanders, D. B. Sasaki, S. Shioya, Y. Tasca, L. Taylor, J. E. TI The cosmic evolution survey (COSMOS): A large-scale structure at z=0.73 and the relation of galaxy morphologies to local environment SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : clusters : general; galaxies : evolution; large-scale structure of universe; surveys ID HUBBLE-SPACE-TELESCOPE; WIDE-FIELD SURVEY; MASS-TEMPERATURE RELATION; DENSITY RELATION; S0 GALAXIES; ADVANCED CAMERA; DARK-MATTER; CLUSTERS; REDSHIFT; SAMPLE AB We have identified a large-scale structure at z similar or equal to 0.73 in the COSMOS field, coherently described by the distribution of galaxy photometric redshifts, an ACS weak- lensing convergence map, and the distribution of extended X- ray sources in a mosaic of XMM- Newton observations. The main peak seen in these maps corresponds to a rich cluster with T-X = 3.51(-0.46)(+0.60) keV and L-X =( 1.56 +/- 0.04)x10(44) ergs s(-1) ( 0.1-2.4 keV band). We estimate an X- ray mass within r(500) corresponding to M-500 similar or equal to 1.6x 10(14) M-circle dot and a total lensing mass ( extrapolated by fitting a NFW profile) M-NFW =(6 +/- 3)x 10(15) M-circle dot. We use an automated morphological classification of all galaxies brighter than I-AB = 24 over the structure area to measure the fraction of early-type objects as a function of local projected density Sigma(10), based on photometric redshifts derived from ground-based deep multiband photometry. We recover a robust morphology-density relation at this redshift, indicating, for comparable local densities, a smaller fraction of early-type galaxies than today. Interestingly, this difference is less strong at the highest densities and becomes more severe in intermediate environments. We also find, however, local "inversions'' of the observed global relation, possibly driven by the large-scale environment. In particular, we find direct correspondence of a large concentration of disk galaxies to ( the colder side of) a possible shock region detected in the X- ray temperature map and surface brightness distribution of the dominant cluster. We interpret this as potential evidence of shock-induced star formation in existing galaxy disks, during the ongoing merger between two subclusters.Our analysis reveals the value of combining various measures of the projected mass density to locate distant structures and their potential for elucidating the physical processes at work in the transformation of galaxy morphologies. C1 Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. Max Planck Inst Astrophys, D-85748 Garching, Germany. Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. Univ Padua, Dipartmento Astron, I-35100 Padua, Italy. Ist Astrofis Spaziale & Fis Cosm, INAF, Sez Milano, I-20133 Milan, Italy. CALTECH, Pasadena, CA 91125 USA. Univ Hawaii, Honolulu, HI 96822 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Tohoku Univ, Grad Sch Sci, Inst Astron, Sendai, Miyagi 9808578, Japan. Ehime Univ, Grad Sch Sci, Dept Phys, Matsuyama 9808577, Japan. Large Binocular Telescope Observ, Tucson, AZ 85721 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Osservatorio Astron Bologna, INAF, Bologna, Italy. Astrophys Lab, F-13376 Marseille 12, France. Univ Paris 06, CNRS, Inst Astrophys, UMR7095, F-75014 Paris, France. Jet Propuls Lab, Pasadena, CA 91109 USA. RP Guzzo, L (reprint author), Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. RI Kneib, Jean-Paul/A-7919-2015; Comastri, Andrea/O-9543-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Comastri, Andrea/0000-0003-3451-9970; Koekemoer, Anton/0000-0002-6610-2048; Brusa, Marcella/0000-0002-5059-6848 NR 56 TC 53 Z9 53 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 254 EP 269 DI 10.1086/516588 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000017 ER PT J AU McCracken, HJ Peacock, JA Guzzo, L Capak, P Porciani, C Scoville, N Aussel, H Finoguenov, A James, JB Kitzbichler, MG Koekemoer, A Leauthaud, A Le Fevre, O Massey, R Mellier, Y Mobasher, B Norberg, P Rhodes, J Sanders, DB Sasaki, SS Taniguchi, Y Thompson, DJ White, SDM El-Zant, A AF McCracken, H. J. Peacock, J. A. Guzzo, L. Capak, P. Porciani, C. Scoville, N. Aussel, H. Finoguenov, A. James, J. B. Kitzbichler, M. G. Koekemoer, A. Leauthaud, A. Le Fevre, O. Massey, R. Mellier, Y. Mobasher, B. Norberg, P. Rhodes, J. Sanders, D. B. Sasaki, S. S. Taniguchi, Y. Thompson, D. J. White, S. D. M. El-Zant, A. TI The angular correlations of galaxies in the COSMOS field SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; dark matter; galaxies : evolution; galaxies : formation; large-scale structure of universe; surveys ID DEEP FIELDS; EVOLUTION AB We present measurements of the two-point galaxy angular correlation function w(theta) in the COSMOS field. Independent determinations of w( theta) as a function of magnitude limit are presented for both the Hubble Space Telescope ( HST) ACS catalog and also the ground-based data from Subaru and the Canada-France-Hawaii Telescope. Despite having significantly different masks, these three determinations agree well. At bright magnitudes ( I-AB < 22), our data generally match very well with existing measurements and with mock catalogs based on the semianalytic galaxy formation calculations of Kitzbichler & White ( 2007) from the Millennium Simulation. The exception is that our result is at the upper end of the expected cosmic variance scatter for theta > 10', which we attribute to a particularly rich structure known to exist at z similar or equal to 0.8. For fainter samples, however, the level of clustering is somewhat higher than reported by some previous studies; in all three catalogs we find w(theta=1')similar or equal to 0.014 at a median I-AB magnitude of 24. At these very faintest magnitudes, our measurements agree well with the latest determinations from the Canada-France Legacy Survey. This level of clustering is approximately double what is predicted by the semianalytic catalogs ( at all angles). The semianalytic results allow an estimate of cosmic variance, which is too small to account for the discrepancy. We therefore conclude that the mean amplitude of clustering at this level is higher than previously estimated. C1 Univ Paris 06, CNRS, Inst Astrophys, UMR 7095, F-75014 Paris, France. Observ Paris, LERMA, F-75014 Paris, France. Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. Max Planck Inst Astrophys, D-85748 Garching, Germany. CALTECH, Pasadena, CA 91125 USA. ETH, Dept Phys, CH-8093 Zurich, Switzerland. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Astrophys Lab, F-13376 Marseille 12, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. Tohoku Univ, Grad Sch Sci, Inst Astron, Sendai, Miyagi 9808578, Japan. Ehime Univ, Grad Sch Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. CALTECH, Opt Observ, Pasadena, CA 91125 USA. Univ Toronto, Canadian Inst Theoret Astrophys, McLennan Labs, Toronto, ON M5S 3H8, Canada. RP McCracken, HJ (reprint author), Univ Paris 06, CNRS, Inst Astrophys, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France. RI Le Fevre, Olivier/G-7389-2011; OI Koekemoer, Anton/0000-0002-6610-2048 NR 18 TC 44 Z9 44 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 314 EP 319 DI 10.1086/518693 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000021 ER PT J AU Scarlata, C Carollo, CM Lilly, S Sargent, MT Feldmann, R Kampczyk, P Porciani, C Koekemoer, A Scoville, N Kneib, JP Leauthaud, A Massey, R Rhodes, J Tasca, L Capak, P Maier, C McCracken, HJ Mobasher, B Renzini, A Taniguchi, Y Thompson, D Sheth, K Ajiki, M Aussel, H Murayama, T Sanders, DB Sasaki, S Shioya, Y Takahashi, M AF Scarlata, C. Carollo, C. M. Lilly, S. Sargent, M. T. Feldmann, R. Kampczyk, P. Porciani, C. Koekemoer, A. Scoville, N. Kneib, J.-P. Leauthaud, A. Massey, R. Rhodes, J. Tasca, L. Capak, P. Maier, C. McCracken, H. J. Mobasher, B. Renzini, A. Taniguchi, Y. Thompson, D. Sheth, K. Ajiki, M. Aussel, H. Murayama, T. Sanders, D. B. Sasaki, S. Shioya, Y. Takahashi, M. TI COSMOS morphological classification with the Zurich Estimator of Structural Types (ZEST) and the evolution since z=1 of the luminosity function of early, disk, and irregular galaxies SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; dark matter; galaxies : evolution; galaxies : formation; large-scale structure of universe; surveys ID DIGITAL SKY SURVEY; REDSHIFT SURVEY; QUANTITATIVE MORPHOLOGY; SURFACE BRIGHTNESS; ELLIPTIC GALAXIES; DISTANT GALAXIES; FIELD; SAMPLE; NEARBY; Z-SIMILAR-TO-2 AB Motivated by the desire to reliably and automatically classify structure of thousands of COSMOS galaxies, we present ZEST, the Zurich Estimator of Structural Types. To classify galaxy structure, ZEST uses ( 1) five nonparametric diagnostics: asymmetry, concentration, Gini coefficient, second-order moment of the brightest 20% of galaxy pixels, and ellipticity; and ( 2) the exponent n of single-Sersic fits to the two-dimensional surface brightness distributions. To fully exploit the wealth of information while reducing the redundancy present in these diagnostics, ZEST performs a principal component ( PC) analysis. We use a sample of similar to 56,000 I-AB <= 24COSMOS galaxies to show that the first three PCs fully describe the key aspects of the galaxy structure, i.e., to calibrate a three-dimensional classification grid of axes PC1, PC2, and PC3. We demonstrate the robustness of the ZEST grid on the z=0 sample of Frei et al. The ZEST classification breaks most of the degeneracy between different galaxy populations that affects morphological classifications based on only some of the diagnostics included in ZEST. As a first application, we present the evolution since z similar to 1 of the luminosity functions (LFs) of COSMOS galaxies of early, disk, and irregular galaxies and, for disk galaxies, of different bulge-to-disk ratios. Overall, we find that the LF up to a redshift z 1 is consistent with a pure luminosity evolution ( of about 0.95 mag at z similar to 0: 7). We highlight, however, two trends that are in general agreement with a downsizing scenario for galaxy formation, i. e., ( 1) a deficit of a factor of about 2 at z similar to 0: 7 of MB > -20: 5 structurally classified early-type galaxies and ( 2) an excess of a factor of about 3, at a similar redshift, of irregular galaxies. C1 ETH, Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland. CALTECH, Pasadena, CA 91125 USA. Astrophys Lab, Marseille 13376, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Inst Astrophys, F-75014 Paris, France. Univ Padua, Dipartmento Astron, I-35122 Padua, Italy. Subaru Telescope, Natl Astron Observ Japan, Hilo, HI 96720 USA. Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Tohoku Univ, Grad Sch Sci, Astron Inst, Sendai, Miyagi 980, Japan. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Ehime Univ, Fac Sci, Dept Phys, Matsuyama, Ehime 790, Japan. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Scarlata, C (reprint author), ETH, Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland. RI Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Maier, Christian/0000-0001-6405-2182; Koekemoer, Anton/0000-0002-6610-2048 NR 55 TC 153 Z9 153 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 406 EP 433 DI 10.1086/516582 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000029 ER PT J AU Sargent, MT Carollo, CM Lilly, SJ Scarlata, C Feldmann, R Kampczyk, P Koekemoer, AM Scoville, N Kneib, JP Leauthaud, A Massey, R Rhodes, J Tasca, LAM Capak, P McCracken, HJ Porciani, C Renzini, A Taniguchi, Y Thompson, DJ Sheth, K AF Sargent, M. T. Carollo, C. M. Lilly, S. J. Scarlata, C. Feldmann, R. Kampczyk, P. Koekemoer, A. M. Scoville, N. Kneib, J.-P. Leauthaud, A. Massey, R. Rhodes, J. Tasca, L. A. M. Capak, P. McCracken, H. J. Porciani, C. Renzini, A. Taniguchi, Y. Thompson, D. J. Sheth, K. TI The evolution of the number density of large disk galaxies in COSMOS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : formation; large-scale structure of universe; surveys ID HUBBLE-DEEP-FIELD; STRUCTURAL PARAMETERS; SURFACE BRIGHTNESS; SECULAR EVOLUTION; SPIRAL GALAXIES; LUMINOSITY FUNCTIONS; SIZE EVOLUTION; BULGES; GEMS; Z-SIMILAR-TO-1 AB We study a sample of approximately 16,500 galaxies with I-ACS; AB <= 22: 5 in the central 38% of the COSMOS field, which are extracted from a catalog constructed from the Cycle 12 ACS F814W COSMOS data set. Structural information on the galaxies is derived by fitting single Sersic models to their two-dimensional surface brightness distributions. In this paper we focus on the disk galaxy population ( as classified by the Zurich Estimator of Structural Types), and investigate the evolution of the number density of disk galaxies larger than approximately 5 kpc between redshift z similar to 1 and the present epoch. Specifically, we use the measurements of the half-light radii derived from the Sersic fits to construct, as a function of redshift, the size function Phi( r1/2; z) of both the total disk galaxy population and of disk galaxies split in four bins of bulge-to-disk ratio. In each redshift bin, the size function specifies the number of galaxies per unit comoving volume and per unit half-light radius r1/2. Furthermore, we use a selected sample of roughly 1800 SDSS galaxies to calibrate our results with respect to the local universe. We find the following: ( 1) The number density of disk galaxies with intermediate sizes (r1/2 similar to 5-7 kpc) remains nearly constant from z similar to 1 to today. Unless the growth and destruction of such systems exactly balanced in the last eight billion years, they must have neither grown nor been destroyed over this period. ( 2) The number density of the largest disks (r1/2 > 7 kpc) decreases by a factor of about 2 out to z similar to 1. ( 3) There is a constancy-or even slight increase-in the number density of large bulgeless disks out to z similar to 1; the deficit of large disks at early epochs seems to arise from a smaller number of bulged disks. Our results indicate that the bulk of the large disk galaxy population has completed its growth by z similar to 1 and support the theory that secular evolution processes produce-or at least add stellar mass to-the bulge components of disk galaxies. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. CALTECH, Pasadena, CA 91125 USA. Univ Hawaii, Honolulu, HI 96822 USA. Astrophys Lab, Marseille 13376, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Paris 06, CNRS, Inst Astrophys, UMR 7095, F-75014 Paris, France. Observ Paris, LERMA, F-75014 Paris, France. Univ Padua, Dept Astron, I-35122 Padua, Italy. Ehime Univ, Grad Sch Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. CALTECH, Pasadena, CA 91125 USA. Univ Arizona, Large Binocular Tel Observ, Tucson, AZ 85721 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Sargent, MT (reprint author), ETH, Dept Phys, CH-8093 Zurich, Switzerland. RI Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Koekemoer, Anton/0000-0002-6610-2048 NR 47 TC 70 Z9 70 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 434 EP 455 DI 10.1086/516584 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000030 ER PT J AU Zamojski, MA Schiminovich, D Rich, RM Mobasher, B Koekemoer, AM Capak, P Taniguchi, Y Sasaki, SS McCracken, HJ Mellier, Y Bertin, E Aussel, H Sanders, DB Le Fevre, O Ilbert, O Salvato, M Thompson, DJ Kartaltepe, JS Scoville, N Barlow, TA Forster, K Friedman, PG Martin, DC Morrissey, P Neff, SG Seibert, M Small, T Wyder, TK Bianchi, L Donas, J Heckman, TM Lee, YW Madore, BF Milliard, B Szalay, AS Welsh, BY Yi, SK AF Zamojski, M. A. Schiminovich, D. Rich, R. M. Mobasher, B. Koekemoer, A. M. Capak, P. Taniguchi, Y. Sasaki, S. S. McCracken, H. J. Mellier, Y. Bertin, E. Aussel, H. Sanders, D. B. Le Fevre, O. Ilbert, O. Salvato, M. Thompson, D. J. Kartaltepe, J. S. Scoville, N. Barlow, T. A. Forster, K. Friedman, P. G. Martin, D. C. Morrissey, P. Neff, S. G. Seibert, M. Small, T. Wyder, T. K. Bianchi, L. Donas, J. Heckman, T. M. Lee, Y.-W. Madore, B. F. Milliard, B. Szalay, A. S. Welsh, B. Y. Yi, S. K. TI Deep GALEX imaging of the COSMOS HST field: A first look at the morphology of z similar to 0.7 star-forming galaxies SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : evolution; galaxies : fundamental parameters; surveys ID DIGITAL SKY SURVEY; COMPACT BLUE GALAXIES; ULTRAVIOLET LUMINOSITY DENSITY; AUTOFIB REDSHIFT SURVEY; FORMATION HISTORIES; INFRARED GALAXIES; ELLIPTIC GALAXIES; LOCAL UNIVERSE; STELLAR MASS; EVOLUTION-EXPLORER AB We present a study of the morphological nature of redshift z similar to 0: 7 star-forming galaxies using a combination of HST ACS, GALEX, and ground-based images of the COSMOS field. Our sample consists of 8146 galaxies, 5777 of which are detected in the GALEX near-ultraviolet band ( 2310 8 or similar to 1360 8 rest frame) down to a limiting magnitude of 25.5 ( AB), and all of which have a brightness of F814W( HST) < 23 mag and photometric redshifts in the range 0: 55 < z < 0: 8. We make use of the UV to estimate star formation rates, correcting for the effect of dust using the UV slope, and of the ground-based multiband data to calculate masses. For all galaxies in our sample, we compute, from the ACS F814W images, their concentration ( C), asymmetry ( A), and clumpiness ( S), as well as their Gini coefficient ( G) and the second moment of the brightest 20% of their light ( M-20). We observe a bimodality in the galaxy population in asymmetry and in clumpiness, although the separation is most evident when either of those parameters is combined with a concentration-like parameter ( C, G, or M20). We further show that this morphological bimodality has a strong correspondence with the FUV-g color bimodality and conclude that UV-optical color predominantly evolves concurrently with morphology. We observe many of the most star-forming galaxies to have morphologies approaching that of early-type galaxies, and we interpret this as evidence that strong starburst events are linked to bulge growth and constitute a process through which galaxies can be brought from the blue to the red sequence while simultaneously modifying their morphology accordingly. We conclude that the red sequence has continued growing at z <= 0. 7. We also observe z similar to 0: 7 galaxies to have physical properties similar to that of local galaxies, except for higher star formation rates. Whence we infer that the dimming of star- forming galaxies is responsible for most of the evolution in star formation rate density since that redshift, although our data are also consistent with a mild number evolution. C1 Columbia Univ, Dept Astron, New York, NY 10027 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. CALTECH, Pasadena, CA 91125 USA. Tohoku Univ, Inst Astron, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Lab Astrophys Marseille, F-13376 Marseille 12, France. CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Lab Astron & Solar Phys, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Zamojski, MA (reprint author), Columbia Univ, Dept Astron, MC2457,550 W 120th St, New York, NY 10027 USA. EM michel@astro.columbia.edu; ds@astro.columbia.edu RI Le Fevre, Olivier/G-7389-2011; OI Koekemoer, Anton/0000-0002-6610-2048 NR 92 TC 101 Z9 101 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 468 EP 493 DI 10.1086/516593 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000032 ER PT J AU Scarlata, C Carollo, CM Lilly, SJ Feldmann, R Kampczyk, P Renzini, A Cimatti, A Halliday, C Daddi, E Sargent, MT Koekemoer, A Scoville, N Kneib, JP Leauthaud, A Massey, R Rhodes, J Tasca, L Capak, P McCracken, HJ Mobasher, B Taniguchi, Y Thompson, D Ajiki, M Aussel, H Murayama, T Sanders, DB Sasaki, S Shioya, Y Takahashi, M AF Scarlata, C. Carollo, C. M. Lilly, S. J. Feldmann, R. Kampczyk, P. Renzini, A. Cimatti, A. Halliday, C. Daddi, E. Sargent, M. T. Koekemoer, A. Scoville, N. Kneib, J.-P. Leauthaud, A. Massey, R. Rhodes, J. Tasca, L. Capak, P. McCracken, H. J. Mobasher, B. Taniguchi, Y. Thompson, D. Ajiki, M. Aussel, H. Murayama, T. Sanders, D. B. Sasaki, S. Shioya, Y. Takahashi, M. TI The redshift evolution of early-type galaxies in COSMOS: Do massive early-type galaxies form by dry mergers? SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : formation; galaxies : structure ID DIGITAL SKY SURVEY; COLOR-MAGNITUDE RELATION; LUMINOUS RED GALAXIES; STELLAR POPULATIONS; ELLIPTIC GALAXIES; STAR-FORMATION; CLUSTERS; GEMS; DISTRIBUTIONS; BRIGHTNESS AB We study the evolution since z similar to 1 of the rest-frame B luminosity function of ETGs in similar to 0.7 deg(2) in the COSMOS field. In order to identify all progenitors of local ETGs we construct the sample of high-z galaxies using two complementary criteria: ( 1) a morphological selection based on the Zurich Estimator of Structural Types and ( 2) a photometric selection based on the galaxy properties in the ( U-V) -M-V color-magnitude diagram. We furthermore constrain both samples so as to ensure that the selected progenitors of ETGs are compatible with evolving into systems that obey the mu(B)-r(hl) Kormendy relation. Assuming the luminosity evolution derived from studies of the fundamental plane for high-z ETGs, our analysis shows no evidence for a decrease in the number density of the most massive ETGs out to z similar to 0: 7: both the morphologically and the photometrically selected subsamples show no evolution in the number density of bright ( similar to L > 2: 5L *) ETGs. Allowing for different star formation histories, and cosmic variance, we estimate amaximum decrease in the number density of massive galaxies at that redshift of similar to 30%. We observe, however, in both the photometric and morphological samples, a deficit of up to about 2-3 of fainter ETGs over the same cosmic period. Our results argue against a significant contribution of recent dissipationless ``dry'' mergers to the formation of the most massive ETGs. We suggest that the mass growth in low-luminosity ETGs can be explained with a conversion from z similar to 0: 7 to z 0 of blue, irregular, and disk galaxies into low- and intermediate-mass ``red'' ETGs, possibly also through gas-rich mergers. C1 Swiss Fed Inst Technol, Dept Phys, ETH, CH-8093 Zurich, Switzerland. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. CALTECH, Pasadena, CA 91125 USA. Lab Astrophys Marseille, F-13376 Marseille 12, France. Jet Prop Lab, Pasadena, CA 91109 USA. Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. Natl Astron Observ, Subaru Telescope, Hilo, HI 96720 USA. Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. Tohoku Univ, Inst Astron, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Ehime Univ, Dept Phys, Grad Sch Sci & Engn, Matsuyama, Ehime, Japan. RP Scarlata, C (reprint author), Swiss Fed Inst Technol, Dept Phys, ETH, CH-8093 Zurich, Switzerland. RI Daddi, Emanuele/D-1649-2012; Kneib, Jean-Paul/A-7919-2015; OI Daddi, Emanuele/0000-0002-3331-9590; Kneib, Jean-Paul/0000-0002-4616-4989; Koekemoer, Anton/0000-0002-6610-2048 NR 64 TC 119 Z9 120 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2007 VL 172 IS 1 BP 494 EP 510 DI 10.1086/517972 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205NW UT WOS:000249122000033 ER PT J AU Hains, JC Chen, LWA Taubman, BF Doddridge, BG Dickerson, RR AF Hains, J. C. Chen, L.-W. A. Taubman, B. F. Doddridge, B. G. Dickerson, R. R. TI A, side-by-side comparison of filter-based PM2.5 measurements at a suburban site: A closure study SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE aerosol sampling; chemical speciation; PM2.5; comparison study; filter sampling ID SAN-JOAQUIN VALLEY; FEDERAL REFERENCE METHOD; FINE PARTICULATE MATTER; SPECIATION TRENDS NETWORK; EASTERN US CITIES; CARBON MEASUREMENTS; ORGANIC AEROSOL; UNITED-STATES; BALTIMORE SUPERSITE; PARTICLE CONCENTRATION AB Assessing the effects of air quality on public health and the environment requires reliable measurement Of PM2.5 mass and its chemical components. This study seeks to evaluate PM2.5 measurements that are part of a newly established national network by comparing them with more versatile sampling systems. Experiments were carried out during 2002 at a suburban site in Maryland, United States, where two samplers from the US Environmental Protection Agency (US EPA) Speciation Trends Network: Met One Speciation Air Sampling System-STNs and Thermo Scientific Reference Ambient Air Sampler-STNR, two Desert Research Institute Sequential Filter Samplers-DRIF, and a continuous TEOM monitor (Thermo Scientific Tapered Element Oscillating Microbalance, 1400a) sampled air in parallel. These monitors differ not only in sampling configuration but also in protocol-specific laboratory analysis procedures. Measurements Of PM2.5 mass and major contributing species (i.e., sulfate, ammonium, organic carbon, and total carbon) were well correlated among the different methods with r-values > 0.8. Despite the good correlations, daily concentrations Of PM2.5 mass and major contributing species were significantly different at the 95% confidence level from 5% to 100% of the time. Larger values of PM2.5 mass and individual species were generally reported from STNR and STNS. These differences can only be partially accounted for by known random errors. Variations in flow design, face velocity, and sampling artifacts possibly influenced the measurement Of PM2.5 speciation and mass closure. Statistical tests indicate that the current uncertainty estimates used in the STN and DRI network may underestimate the actual uncertainty. (c) 2007 Elsevier Ltd. All rights reserved. C1 Univ Maryland, Dept Chem, College Pk, MD 20742 USA. Univ Nevada, Desert Res Inst, Div Atmospher Sci, Reno, NV 89506 USA. Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RP Hains, JC (reprint author), Univ Maryland, Dept Chem, College Pk, MD 20742 USA. EM jhains@atmos.umd.edu RI Chen, Lung-Wen/J-5792-2015; Dickerson, Russell/F-2857-2010 OI Chen, Lung-Wen/0000-0002-2311-7506; Dickerson, Russell/0000-0003-0206-3083 NR 76 TC 14 Z9 15 U1 1 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD SEP PY 2007 VL 41 IS 29 BP 6167 EP 6184 DI 10.1016/j.atmosenv.2007.04.008 PG 18 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 214QE UT WOS:000249752400007 ER PT J AU Kokhanovsky, AA Breon, FM Cacciari, A Carboni, E Diner, D Di Nicolantonio, W Grainger, RG Grey, WMF Holler, R Lee, KH Li, Z North, PRJ Sayer, AM Thomas, GE von Hoyningen-Huene, W AF Kokhanovsky, A. A. Breon, F.-M. Cacciari, A. Carboni, E. Diner, D. Di Nicolantonio, W. Grainger, R. G. Grey, W. M. F. Hoeller, R. Lee, K.-H. Li, Z. North, P. R. J. Sayer, A. M. Thomas, G. E. von Hoyningen-Huene, W. TI Aerosol remote sensing over land: A comparison of satellite retrievals using different algorithms and instruments SO ATMOSPHERIC RESEARCH LA English DT Article DE satellite remote sensing; atmospheric optics; aerosols ID SURFACE BIDIRECTIONAL REFLECTANCE; OPTICAL DEPTH; RADIATIVE-TRANSFER; VEGETATION INDEX; ATMOSPHERE; MODIS; SCATTERING; CALIBRATION; VALIDATION; SCIAMACHY AB An inter-comparison study of the aerosol optical thickness (AOT) at 0.55 mu m retrieved using different satellite instruments and algorithms based on the analysis of backscattered solar light is presented for a single scene over central Europe on October 13th, 2005. For the first time comparisons have been performed for as many as six instruments on multiple satellite platforms. Ten different algorithms are briefly discussed and inter-compared. It was found that on the scale of a single pixel there can be large differences in AOT retrieved over land using different retrieval techniques and instruments. However, these differences are not as pronounced for the average AOT over land. For instance, the average AOT at 0.55 mu m for the area 7-12E, 49-53N was equal to 0.14 for MISR, NASA MODIS and POLDER algorithms. It is smaller by 0.01 for the ESA MERIS aerosol product and larger by 0.04 for the MERIS BAER algorithm. AOT as derived using AATSR gives on average larger values as compared to all other instruments, while SCIAMACHY retrievals underestimate the aerosol loading. These discrepancies are explained by uncertainties in a priori assumptions used in the different algorithms and differences in the sensor characteristics. Validation against AERONET shows that MERIS provides the most accurate AOT retrievals for this scene. (C) 2007 Elsevier B.V. All rights reserved. C1 Inst environm Phys, D-28334 Bremen, Germany. CEA, DSM, LSCE, ALb Sci Climat & Environm, F-91191 Gif Sur Yvette, France. CNR, ISAC, Inst Atmospher & Climat Sci, I-40129 Bologna, Italy. Clarendon Lab, Oxford OX1 3PU, England. CALTECH, JPL, Pasadena, CA 91109 USA. Swansea Univ, Sch Environm & Soc, Climate & Land Surface Syst Interact Ctr, Swansea SA2 8PP, W Glam, Wales. Fed Environm Agcy, A-1190 Vienna, Austria. Univ Maryland, Earth Syst Sci Interdiscplinary Ctr, College Pk, MD 20742 USA. RP Kokhanovsky, AA (reprint author), Inst environm Phys, O Hahn Allee 1, D-28334 Bremen, Germany. EM alexk@iup.physik.uni-bremen.de RI Sayer, Andrew/H-2314-2012; Carboni, Elisa/K-9404-2013; Grainger, Roy/E-8823-2011; Li, Zhanqing/F-4424-2010; North, Peter/A-1616-2009; Kokhanovsky, Alexander/C-6234-2016; Breon, Francois-Marie/M-4639-2016; OI Sayer, Andrew/0000-0001-9149-1789; Carboni, Elisa/0000-0002-0236-7856; Grainger, Roy/0000-0003-0709-1315; Li, Zhanqing/0000-0001-6737-382X; North, Peter/0000-0001-9933-6935; Kokhanovsky, Alexander/0000-0001-7370-1164; Breon, Francois-Marie/0000-0003-2128-739X; Lee, Kwon-Ho/0000-0002-0844-5245 NR 54 TC 101 Z9 104 U1 5 U2 30 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD SEP PY 2007 VL 85 IS 3-4 BP 372 EP 394 DI 10.1016/j.atmosres.2007.02.008 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 210UX UT WOS:000249482200008 ER PT J AU Bhatia, AK Landi, E AF Bhatia, A. K. Landi, E. TI Atomic data and spectral line intensities for MgIX SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID BE-LIKE IONS; EXTREME-ULTRAVIOLET SPECTRUM; ELECTRON-IMPACT-EXCITATION; BERYLLIUM-LIKE IONS; COLLISION STRENGTHS; EMISSION-LINES; TRANSITION-PROBABILITIES; OSCILLATOR-STRENGTHS; RATE COEFFICIENTS; CROSS-SECTIONS AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Mg IX. The configurations used are 2s(2), 2s2p, 2P(2), 2l3l', 2l4l' and 2s5l, with l = s, p and l' = s, p, d giving rise to 92 fine-structure levels in intermediate coupling. Collision strengths are calculated at seven incident energies (6, 12, 25, 50, 75, 100, and 125 Ry) for the transitions within the three lowest configurations, and five incident energies (25, 50, 75, 100, and 125 Ry) for transitions between the ground configuration and the n = 3,4,5 configurations. Calculations have been carried out using the distorted wave approximation. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates of the present work, and R-Matrix results for the 2s(2), 2s2p, 2p(2) configurations available in the literature, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(8)-10(14) cm(-1) at an electron temperature of log T-e (K) = 6.0, corresponding to the maximum abundance of Mg IX Spectral line intensities are calculated, and their diagnostic relevance is discussed. Observed line ratios indicate electron temperatures of the emitting plasma which agree with log T-e (K) = 6.0. This dataset will be made available in the next version of the CHIANTI database. (c) 2007 Elsevier Inc. All rights reserved. C1 USN, Res Lab, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. ARTEP Inc, Columbia, MD 21044 USA. RP Landi, E (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM Landi@poppeo.nrl.navy.mil RI Landi, Enrico/H-4493-2011 NR 37 TC 6 Z9 6 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 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD SEP PY 2007 VL 93 IS 5 BP 742 EP 778 DI 10.1016/j.adt.2007.06.001 PG 37 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA 205IH UT WOS:000249106700004 ER PT J AU Hecht, SB Saatchi, SS AF Hecht, Susanna B. Saatchi, Sassan S. TI Globalization and forest resurgence: Changes in forest cover in El Salvador SO BIOSCIENCE LA English DT Article DE deforestation; globalization; remittances; forest recovery; Central America ID ENVIRONMENTAL SERVICES HELP; ADJUSTED VEGETATION INDEX; COUNTRYSIDE BIOGEOGRAPHY; SECONDARY FORESTS; COSTA-RICA; DEVELOPING-COUNTRIES; BRAZILIAN AMAZON; REDUCE POVERTY; LATIN-AMERICA; SHADE COFFEE AB Globalization is often associated with deforestation, but its impacts on forest recovery are less known. We analyzed socioeconomic data, land-use surveys, and satellite imagery to monitor changes in woody cover in El Salvador from the early 1990s to the presen't. Even where rural population density exceeded 250 people per square kilometer, we documented a 22% increase in the area with more than 30% tree cover, and a 7% increase in the area with more than 60% tree cover. Woodland resurgence reflected processes including civil war, retraction of the agricultural frontier, and international migration and associated remittances. Agrarian reform, structural adjustment, and emerging environmental ideas also played a role in woodland dynamics. Remittances may be especially important for woodland recovery in El Salvador, enabling people in rural areas to buy food without all of them needing to grow and sell it. This study adds to our understanding of the complexity of land-use change in emerging globalized economies and of potential conservation approaches for inhabited landscapes. C1 Univ Calif Los Angeles, Sch Publ Affairs, Los Angeles, CA 90095 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91011 USA. RP Hecht, SB (reprint author), Univ Calif Los Angeles, Sch Publ Affairs, Los Angeles, CA 90095 USA. EM sbhecht@ucla.edu; sassan.saatchi@jpl.nasa.gov NR 69 TC 70 Z9 72 U1 3 U2 23 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD SEP PY 2007 VL 57 IS 8 BP 663 EP 672 DI 10.1641/B570806 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 211FW UT WOS:000249510700008 ER PT J AU Senocak, I Ackerman, AS Kirkpatrick, MP Stevens, DE Mansour, NN AF Senocak, Inanc Ackerman, Andrew S. Kirkpatrick, Michael P. Stevens, David E. Mansour, Nagi N. TI Study of near-surface models for large-eddy simulations of a neutrally stratified atmospheric boundary layer SO BOUNDARY-LAYER METEOROLOGY LA English DT Article DE atmospheric boundary layer; dynamic models; large-eddy simulations; near-surface models ID SUBGRID-SCALE MODEL; TURBULENT FLOWS; WALL; FLUXES; LES AB In large-eddy simulations (LES) of the atmospheric boundary layer (ABL), nearsurface models are often used to supplement subgrid-scale (SGS) turbulent stresses when a major fraction of the energetic scales within the surface layer cannot be resolved with the temporal and spatial resolution at hand. In this study, we investigate the performance of both dynamic and non-dynamic eddy viscosity models coupled with near-surface models in simulations of a neutrally stratified ABL. Two near-surface models that are commonly used in LES of the atmospheric boundary layer are considered. Additionally, a hybrid Reynolds-averaged/LES eddy viscosity model is presented, which uses Prandtl's mixing length model in the vicinity of the surface, and blends in with the dynamic Smagorinsky model away from the surface. Present simulations show that significant portions of the modelled turbulent stresses are generated by the near-surface models, and they play a dominant role in capturing the expected logarithmic wind profile. Visualizations of the instantaneous vorticity field reveal that flow structures in the vicinity of the surface depend on the choice of the near-surface model. Among the three near-surface models studied, the hybrid eddy viscosity model gives the closest agreement with the logarithmic wind profile in the surface layer. It is also observed that high levels of resolved turbulence stresses can be maintained with the so-called canopy stress model while producing good agreement with the logarithmic wind profile. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Stanford Univ, NASA Ames, Ctr Turbulence Res, Stanford, CA 94305 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Univ Sydney, Sch Aerosp Mech & Mechatron Engn, Sydney, NSW 2006, Australia. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Senocak, I (reprint author), Los Alamos Natl Lab, Mail Stop K575,POB 1663, Los Alamos, NM 87545 USA. EM senocak@lanl.gov RI Ackerman, Andrew/D-4433-2012; OI Ackerman, Andrew/0000-0003-0254-6253; Kirkpatrick, Michael/0000-0002-7157-6440 NR 42 TC 12 Z9 12 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0006-8314 J9 BOUND-LAY METEOROL JI Bound.-Layer Meteor. PD SEP PY 2007 VL 124 IS 3 BP 405 EP 424 DI 10.1007/s10546-007-9181-x PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 195MX UT WOS:000248417400005 ER PT J AU Abdeldayem, H Frazier, DO AF Abdeldayem, Hossin Frazier, Donald O. TI Optical computing: Need and challenge SO COMMUNICATIONS OF THE ACM LA English DT Article C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Abdeldayem, H (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM hossin.a.abdeldayem@nasa.gov; donald.o.frazier@nasa.gov NR 11 TC 7 Z9 7 U1 0 U2 1 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036 USA SN 0001-0782 J9 COMMUN ACM JI Commun. ACM PD SEP PY 2007 VL 50 IS 9 BP 60 EP 62 DI 10.1145/1284621.1284649 PG 3 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 206XB UT WOS:000249215100015 ER PT J AU Kaneko, H Bey, KS Daffer, PZ Toghaw, P AF Kaneko, Hideaki Bey, Kim S. Daffer, Peter Z. Toghaw, Puntip TI Error analysis of the p-version discontinuous Galerkin method for heat transfer in built-up structures SO COMMUNICATIONS ON PURE AND APPLIED ANALYSIS LA English DT Article DE discontinuous Galerkin method; heat equations ID FINITE-ELEMENT-METHOD; PARABOLIC PROBLEMS; H-VERSION; 1-DIMENSION AB In this paper, we provide an error analysis for the p-version of the discontinuous Calerkin finite element method for a class of heat transfer problems in built-up structures. Also, a general form of the matrix associated with the discretization of time variable using the p-finite element basis functions is established. Many interesting properties of this matrix are obtained. Numerical examples are provided in the last section. C1 Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. NASA, Langley Res Ctr, Thermal Struct Branch, Struct Div, Hampton, VA 23681 USA. Northrup Grumman Space Technol, Warner Robins, GA 31088 USA. Mahidol Univ, Dept Math, Bangkok 10700, Thailand. RP Kaneko, H (reprint author), Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. EM hkaneko@odu.edu; kim.s.bey@nasa.gov; Peter.Daffer.Ctr@ROBINS.AF.MIL; g4737882@student.mahidol.ac.th NR 14 TC 0 Z9 0 U1 0 U2 0 PU AMER INST MATHEMATICAL SCIENCES PI SPRINGFIELD PA PO BOX 2604, SPRINGFIELD, MO 65801-2604 USA SN 1534-0392 J9 COMMUN PUR APPL ANAL JI Commun. Pure Appl. Anal PD SEP PY 2007 VL 6 IS 3 BP 719 EP 740 PG 22 WC Mathematics, Applied; Mathematics SC Mathematics GA 172IG UT WOS:000246796900008 ER PT J AU Peck, JA Jones, RA Pang, SS Li, GQ Smith, BH AF Peck, Jerry Alan Jones, Randy A. Pang, Su-Seng Li, Guoqiang Smith, Brett H. TI UV-cured FRP joint thickness effect on coupled composite pipes SO COMPOSITE STRUCTURES LA English DT Article; Proceedings Paper CT Annual Conference of the Society-for-the-Advancement-of-Material-and-Process-Engineering CY 2004 CL Long Beach, CA SP Soc Advancement Mat & Proc Engn DE UV curing; light intensity; FRP; composite pipes; joining ID PHOTOPOLYMERIZATION REACTIONS; LIGHT-INTENSITY; KINETICS; CHAIN AB In this study, 36 FRP composite pipes were joined with various layers of fiber-reinforced UV curing vinylester. Twelve of the composite pipes were joined with an eight-layer weld, 12 with five layers and 12 with three layers; each configuration used exactly one layer of E-glass woven fabric with the remaining layers being comprised of chopped strand mat of various widths. The joined pipes were cured with UV lamps at 80 milli-Watts per square centimeter. The mechanical properties of the cured pipe joints were evaluated by conducting internal pressure testing and simply supported four-point bending testing. The effect of joint thickness on the internal pressure rating, ultimate bending load, and stiffness was evaluated to determine the role of joint thickness in under-curing of UV curing vinylesters. There was a direct correlation observed between joint thickness and internal pressure rating. The five-layer and three-layer joints each performed better than the eight-layer joint in bursting. The mechanism for variation in the residual properties was found to be the degree of cure and was validated by finite element analysis that utilized a composite model that simulates variable cure. (C) 2006 Elsevier Ltd. All rights reserved. C1 Louisiana State Univ, Dept Mech Engn, Baton Rouge, LA 70803 USA. EDO Fiber Sci, Salt Lake City, UT 84116 USA. NASA, George C Marshall Space Flight Ctr, Proc & Mfg Dept, Huntsville, AL 35812 USA. RP Peck, JA (reprint author), Louisiana State Univ, Dept Mech Engn, Baton Rouge, LA 70803 USA. EM japeck@me.lsu.edu NR 13 TC 6 Z9 6 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 J9 COMPOS STRUCT JI Compos. Struct. PD SEP PY 2007 VL 80 IS 2 BP 290 EP 297 DI 10.1016/j.compstruct.2006.05.009 PG 8 WC Materials Science, Composites SC Materials Science GA 177OV UT WOS:000247163300012 ER PT J AU Jegley, DC AF Jegley, Dawn C. TI Improving strength of postbuckled panels through stitching SO COMPOSITE STRUCTURES LA English DT Article DE graphite-epoxy; aircraft; composite; stitching; buckling; postbuckling; debond ID BEHAVIOR AB The behavior of blade-stiffened graphite-epoxy panels with impact damage is examined to determine the effect of adding through-the-thickness stitches in the stiffener flange-to-skin interface. The influence of stitches is evaluated by examining buckling and failure for panels with failure loads up to 3.5 times greater than buckling loads. Analytical and experimental results from four configurations of panel specimens are presented. For each configuration, two panels were manufactured with skin and flanges held together with through-the-thickness stitches introduced prior to resin infusion and curing and one panel was manufactured with no stitches holding the flange to the skin. No mechanical fasteners were used for the assembly of any of these panels. Panels with and without low-speed impact damage were loaded to failure in compression. Buckling and failure modes are discussed. Stitching had little effect on buckling loads but increased the failure loads of impact-damaged panels by up to 30%. Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Jegley, DC (reprint author), NASA, Langley Res Ctr, Mail Stop 190, Hampton, VA 23681 USA. EM dawn.c.jegley@nasa.gov NR 21 TC 5 Z9 6 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 J9 COMPOS STRUCT JI Compos. Struct. PD SEP PY 2007 VL 80 IS 2 BP 298 EP 306 DI 10.1016/j.compstruct.2006.05.024 PG 9 WC Materials Science, Composites SC Materials Science GA 177OV UT WOS:000247163300013 ER PT J AU Flanagin, M Grenotton, A Ratcliff, J Shaw, KB Sample, J Abdelguerfi, M AF Flanagin, Maik Grenotton, Aurelien Ratcliff, Jay Shaw, Kevin B. Sample, John Abdelguerfi, Mahdi TI Hydraulic splines - A hybrid approach to modeling river channel geometries SO COMPUTING IN SCIENCE & ENGINEERING LA English DT Article AB The hydraulic spline algorithm generates irregular 2D channel grids from highly accurate cross-sectional survey data at any desired resolution, facilitating its integration with high-density light detection and ranging (lidar) data. C1 USA, Corps Engineers, New Orleans, LA USA. Ecole Cent, Nantes, France. Naval Res Lab, Digital Mapping Charting & Geodesy Anal Program, Washington, DC 20375 USA. Stennis Space Ctr, Naval Res Lab, Mississippi State, MS USA. Univ New Orleans, Dept Comp Sci, New Orleans, LA 70148 USA. RP Flanagin, M (reprint author), USA, Corps Engineers, New Orleans, LA USA. EM maik.c.flanagin@mvn02.usace.army.mil; jay.ratcliff@usace.army.mil; shaw@nrlssc.navy.mil; sample@nrlssc.navy.mil; mahdi@cs.uno.edu NR 22 TC 3 Z9 3 U1 1 U2 4 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1521-9615 J9 COMPUT SCI ENG JI Comput. Sci. Eng. PD SEP-OCT PY 2007 VL 9 IS 5 BP 4 EP 15 DI 10.1109/MCSE.2007.99 PG 12 WC Computer Science, Interdisciplinary Applications SC Computer Science GA 200XV UT WOS:000248797000002 ER PT J AU Brosten, TR Park, JM Evans, AT Rasmussen, K Nellis, GF Klein, SA Feller, JR Salerno, L Gianchandani, YB AF Brosten, Tyler R. Park, Jong M. Evans, Allan T. Rasmussen, Kristian Nellis, Gregory F. Klein, Sanford A. Feller, Jeffery R. Salerno, Louis Gianchandani, Yogesh B. TI A numerical flow model and experimental results of a cryogenic micro-valve for distributed cooling applications SO CRYOGENICS LA English DT Article ID MICROCHANNELS AB This paper describes a steady numerical flow model and experimental gas flow results of a self-encapsulated, piezoelectrically actuated, cryogenic micro-valve for distributed cooling applications. Experimental flow data of the prototype micro-valve design is obtained for various gases at room temperature and for helium at near liquid nitrogen temperature. With a pressure differential of 100 kPa across the inlet and outlet, a prototype micro-valve is shown to modulate the flow of room temperature helium from 1200 to 0 sccm. Numerical flow results and experimental data agree well, with 60% of the data points falling within the range of +/- 10%. (C) 2007 Elsevier Ltd. All rights reserved. C1 Univ Wisconsin, Dept Mech Engn, Madison, WI 53706 USA. Univ Michigan, Dept Elect Engn & Comp Sci, Ann Arbor, MI 48109 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Nellis, GF (reprint author), Univ Wisconsin, Dept Mech Engn, Madison, WI 53706 USA. EM gfnellis@engr.wise.edu NR 19 TC 6 Z9 6 U1 1 U2 10 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 J9 CRYOGENICS JI Cryogenics PD SEP-OCT PY 2007 VL 47 IS 9-10 BP 501 EP 509 DI 10.1016/j.cryogenies.2007.06.002 PG 9 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA 229BX UT WOS:000250777400007 ER PT J AU Spina, AP AF Spina, Anthony P. TI Thermal ecology of juvenile steelhead in a warm-water environment SO ENVIRONMENTAL BIOLOGY OF FISHES LA English DT Article DE behavior; habitat use; temperature preference; temperature tolerance ID TROUT SALMO-GAIRDNERI; RAINBOW-TROUT; PHYSIOLOGICAL PERFORMANCE; TEMPERATURE TOLERANCES; CONSTANT TEMPERATURES; LETHAL TEMPERATURES; CUTTHROAT TROUT; UNITED-STATES; CALIFORNIA; MAXIMA AB How salmonids adjust to the cost of chronic exposure to warm water in nature, particularly in habitats where areas of cold water are unavailable, is largely unknown. In the hot dry climate of southern California, oversummering juvenile steelhead, Oncorhynchus mykiss, can experience a continual warm-water environment. Studies were performed in three streams (34 degrees N) during the summers of 2002-2004 to assess how steelhead (10-28 cm total length) exploit the thermal environment and to develop an understanding of how existing preference and heat tolerance information reported for the species relate to the actual temperatures the local population experiences. Analyses of achievable body temperatures, an index of observed body temperatures, and behavioral time budgets, indicate steelhead did not behaviorally thermoregulate. Findings from associated field surveys suggest areas of cold water were not available. Steelhead held focal points at temperatures (17.4-24.8 degrees C) that were at times higher than the temperature preferences and heat tolerances reported for the species. Oversurnmering juvenile steelhead accept an elevated body temperature and remain active and forage throughout the day, apparently as a means for coping with warm water at the southern extent of their range. The relatively high body temperatures that steelhead accept appear to represent a compromise in exchange for maintaining an expanded geographic (latitudinal) range. (c) Springer Science+Business Media B.V. 2006 C1 Natl Marine Fisheries Serv, Long Beach, CA 90802 USA. RP Spina, AP (reprint author), Natl Marine Fisheries Serv, 501 W Ocean Blvd,Suite 4200, Long Beach, CA 90802 USA. EM anthony.spina@noaa.gov NR 39 TC 17 Z9 21 U1 1 U2 29 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0378-1909 J9 ENVIRON BIOL FISH JI Environ. Biol. Fishes PD SEP PY 2007 VL 80 IS 1 BP 23 EP 34 DI 10.1007/s10641-006-9103-7 PG 12 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 203ZH UT WOS:000249012100004 ER PT J AU Wood, SJ Reschke, MF Sarmiento, LA Clement, G AF Wood, Scott J. Reschke, Millard F. Sarmiento, Laura A. Clement, Gilles TI Tilt and translation motion perception during off-vertical axis rotation SO EXPERIMENTAL BRAIN RESEARCH LA English DT Article DE OVAR; otolith; spatial orientation; multi-sensory integration ID QUALITATIVELY DIFFERENT MECHANISMS; OTOLITH-OCULAR REFLEXES; EYE-MOVEMENT RESPONSES; LINEAR ACCELERATION; SMALL ANGLES; ROLL-TILT; VESTIBULAR INFORMATION; ATTENTIONAL DEMANDS; INTERNAL-MODELS; INERTIAL MOTION AB The effect of stimulus frequency on tilt and translation motion perception was studied during constant velocity off-vertical axis rotation (OVAR), and compared to the effect of stimulus frequency on eye movements. Fourteen healthy subjects were rotated in darkness about their longitudinal axis 10 degrees and 20 degrees off-vertical at 45 degrees/s (0.125 Hz) and 20 degrees off-vertical at 180 degrees/s (0.5 Hz). Perceived motion was evaluated using verbal reports and a joystick capable of recording tilt and translation in both sagittal and lateral planes. Eye movements were also recorded using videography. At the lower frequency, subjects reported the perception of progressing along the edge of a cone, whereas at the higher frequency they had the sensation of progressing along the edge of an upright cylinder. Tilt perception and ocular torsion significantly increased as the tilt angle increased from 10 degrees to 20 degrees at the lower frequency, and then decreased at the higher frequency. The phase lag of ocular torsion increased as a function of frequency, while the phase lag of tilt perception did not change. Horizontal eye movements were small at the lower frequency and showed a phase lead relative to the linear acceleration stimulus. While the phase lead of horizontal eye movements decreased at 0.5 Hz, the phase of translation perception did not vary with stimulus frequency and was similar to the phase of tilt perception during all conditions. A second data set was obtained in 12 subjects to compare motion perception phase when using a simple push-button to indicate nose-up orientation, continuous setting of pitch tilt alone, or continuous setting of tilt and translation in both pitch and roll planes as in the first data set. This set of measurements indicated that in the frequency range studied subjects tend to lead the stimulus when using a push-button task while lagging the stimulus when using a continuous setting of tilt with a joystick. Both amplitude and phase of tilt perception using the joystick were not different whether concentrating on pitch tilt alone or attempting a more complex reporting of tilt and translation in both sagittal and lateral planes. During dynamic linear stimuli in the absence of canal and visual input, a change in stimulus frequency alone elicits similar changes in the amplitude of both self-motion perception and eye movements. However, in contrast to the eye movements, the phase of both perceived tilt and translation motion is not altered by stimulus frequency over this limited range. These results are consistent with the hypothesis that neural processing to distinguish tilt and translation stimuli differs between eye movements and motion perception. C1 NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, Houston, TX 77058 USA. Univ Space Res Assoc, Houston, TX USA. Ctr Rech Cerveau Cognit, CNRS, UPS, UMR 5549, Toulouse, France. RP Wood, SJ (reprint author), NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, 2101 NASA Parkway,Mail Code SK 272, Houston, TX 77058 USA. EM scott.j.wood@nasa.gov NR 61 TC 20 Z9 20 U1 0 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0014-4819 J9 EXP BRAIN RES JI Exp. Brain Res. PD SEP PY 2007 VL 182 IS 3 BP 365 EP 377 DI 10.1007/s00221-007-0994-0 PG 13 WC Neurosciences SC Neurosciences & Neurology GA 209RF UT WOS:000249405000008 PM 17565488 ER PT J AU Warren-Rhodes, KA Rhodes, KL Boyle, LN Pointing, SB Chen, Y Liu, SJ Zhuo, PJ Mckay, CP AF Warren-Rhodes, Kimberley A. Rhodes, Kevin L. Boyle, Linda Ng Pointing, Stephen B. Chen, Yong Liu, Shuangjiang Zhuo, Peijin McKay, Christopher P. TI Cyanobacterial ecology across environmental gradients and spatial scales in China's hot and cold deserts SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE hypolithic; photoautotrophs; hyperarid desert; landscape ecology; patchiness; trigger-transfer-response-pulse framework ID SEMIARID LANDSCAPES; CONCEPTUAL-MODEL; SOIL-MOISTURE; DIVERSITY; CHROOCOCCIDIOPSIS; DESERTIFICATION; MICROORGANISMS; COLONIZATION; CONTINUUM; ECOSYSTEM AB Lithic photoautotrophic communities function as principal primary producers in the world's driest deserts, yet many aspects of their ecology remain unknown. This is particularly true for Asia, where some of the Earth's oldest and driest deserts occur. Using methods derived from plant landscape ecology, we measured the abundance and spatial distribution of cyanobacterial colonization on quartz stony pavement across environmental gradients of rainfall and temperature in the isolated Taklimakan and Qaidam Basin deserts of western China. Colonization within available habitat ranged from 0.37 +/- 0.16% to 12.6 +/- 1.8%, with cold dry desert sites exhibiting the lowest abundance. Variation between sites was most strongly correlated with moisture-related variables and was independent of substrate availability. Cyanobacterial communities were spatially aggregated at multiple scales in patterns distinct from the underlying rock pattern. Site-level differences in cyanobacterial spatial pattern (e.g. mean inter-patch distance) were linked with rainfall, whereas patchiness within sites was correlated with local geology (greater colonization frequency of large rocks) and biology (dispersal during rainfall). We suggest that cyanobacterial patchiness may also in part be self-organized - that is, an outcome of soil water-biological feedbacks. We propose that landscape ecology concepts and models linking desert vegetation, biological feedbacks and ecohydrological processes are applicable to microbial communities. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Hawaii, Coll Agr Forestry & Nat Resource Management, Hilo, HI 96720 USA. Univ Iowa, Dept Mech & Ind Engn, Iowa City, IA USA. Univ Hong Kong, Sch Biol Sci, Hong Kong, Hong Kong, Peoples R China. Chinese Acad Sci, Inst Microbiol, Beijing, Peoples R China. RP Warren-Rhodes, KA (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM kwarren-rhodes@mail.arc.nasa.gov NR 61 TC 38 Z9 40 U1 1 U2 17 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0168-6496 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD SEP PY 2007 VL 61 IS 3 BP 470 EP 482 DI 10.1111/j.1574-6941.2007.00351.x PG 13 WC Microbiology SC Microbiology GA 203GA UT WOS:000248961900008 PM 17672851 ER PT J AU Moissl, C Osman, S La Duc, MT Dekas, A Brodie, E DeSantis, T Venkateswaran, K AF Moissl, Christine Osman, Shariff La Duc, Myron T. Dekas, Anne Brodie, Eoin DeSantis, Tadd Venkateswaran, Kasthuri TI Molecular bacterial community analysis of clean rooms where spacecraft are assembled SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE spacecraft assembly facility; bacterial community analysis; 16S rRNA; clean room; planetary protection; astrobiology ID MICROBIAL-CONTAMINATION; OLIGOTROPHIC MICROORGANISMS; DIVERSITY; ENVIRONMENTS; SURVIVAL; IRRADIATION; STATION; UNIFRAC; SPORES; MARS AB Molecular bacterial community composition was characterized from three geographically distinct spacecraft-associated clean rooms to determine whether such populations are influenced by the surrounding environment or the maintenance of the clean rooms. Samples were collected from facilities at the Jet Propulsion Laboratory (JPL), Kennedy Space Flight Center (KSC), and Johnson Space Center (JSC). Nine clone libraries representing different surfaces within the spacecraft facilities and three libraries from the surrounding air were created. Despite the highly desiccated, nutrient-bare conditions within these clean rooms, a broad diversity of bacteria was detected, covering all the main bacterial phyla. Furthermore, the bacterial communities were significantly different from each other, revealing only a small subset of microorganisms common to all locations (e.g. Sphingomonas, Staphylococcus). Samples from JSC assembly room surfaces showed the greatest diversity of bacteria, particularly within the Alpha- and Gammaproteobacteria and Actinobacteria. The bacterial community structure of KSC assembly surfaces revealed a high presence of proteobacterial groups, whereas the surface samples collected from the JPL assembly facility showed a predominance of Firmicutes. Our study presents the first extended molecular survey and comparison of NASA spacecraft assembly facilities, and provides new insights into the bacterial diversity of clean room environments . C1 CALTECH, Jet Propuls Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Ctr Environm Biotechnol, Berkeley, CA 94720 USA. RP Venkateswaran, K (reprint author), CALTECH, Jet Propuls Lab, Biotechnol & Planetary Protect Grp, MS 89-2,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kjvenkat@jpl.nasa.gov RI Moissl-Eichinger, Christine/A-6682-2015; Brodie, Eoin/A-7853-2008 OI Moissl-Eichinger, Christine/0000-0001-6755-6263; Brodie, Eoin/0000-0002-8453-8435 NR 48 TC 59 Z9 59 U1 1 U2 19 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0168-6496 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD SEP PY 2007 VL 61 IS 3 BP 509 EP 521 DI 10.1111/j.1574-6941.2007.00360.x PG 13 WC Microbiology SC Microbiology GA 203GA UT WOS:000248961900011 PM 17655710 ER PT J AU Tirado, EE Marquette, ML Rivnay, B Brown, DB AF Tirado, E. E. Marquette, M. L. Rivnay, B. Brown, D. B. TI Comparison of lipid peroxidation (LPO) and sperm function after isolating sperm using a density gradient. SO FERTILITY AND STERILITY LA English DT Meeting Abstract CT 63rd Annual Meeting of the American-Society-for-Reproductive-Medicine CY OCT 13-17, 2007 CL Washington, DC SP Amer Soc Reproduct Med C1 Repromedix, Res & Dev, Woburn, MA USA. Univ Texas, Med Branch, Dept Neurosci & Cell Biol, Galveston, TX 77550 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0015-0282 J9 FERTIL STERIL JI Fertil. Steril. PD SEP PY 2007 VL 88 SU 1 BP S305 EP S305 PG 1 WC Obstetrics & Gynecology; Reproductive Biology SC Obstetrics & Gynecology; Reproductive Biology GA 216PC UT WOS:000249889800869 ER PT J AU Wortmann, UG Chernyavsky, B Bernasconi, SM Brunner, B Bottcher, ME Swart, PK AF Wortmann, Ulrich G. Chernyavsky, Boris Bernasconi, Stefano M. Brunner, Benjamin Boettcher, Michael E. Swart, Peter K. TI Oxygen isotope biogeochemistry of pore water sulfate in the deep biosphere: Dominance of isotope exchange reactions with ambient water during microbial sulfate reduction (ODP Site 1130) SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID MARINE-SEDIMENTS; ENVIRONMENTAL SIGNIFICANCE; BACTERIAL REDUCTION; REDUCING BACTERIA; DISSOLVED SULFATE; STABLE SULFUR; FRACTIONATION; MODEL; CARBON; DISPROPORTIONATION AB Microbially mediated sulfate reduction affects the isotopic composition of dissolved and solid sulfur species in marine sediments. Experiments and field data show that the delta O-18(SO4)2- composition is also modified in the presence of sulfate-reducing microorganisms. This has been attributed either to a kinetic isotope effect during the reduction of sulfate to sulfite, cell-internal exchange reactions between enzymatically-activated sulfate (APS), and/or sulfite with cytoplasmic water. The isotopic fingerprint of these processes may be further modified by the cell-external reoxidation of sulfide to elemental sulfur, and the subsequent disproportionation to sulfide and sulfate or by the oxidation of sulfite to sulfate. Here we report delta O-18(SO4)2- values from interstitial water samples of ODP Leg 182 (Site 1130) and provide the mathematical framework to describe the oxygen isotope fractionation of sulfate during microbial sulfate reduction. We show that a purely kinetic model is unable to explain our delta(OSO42-)-O-18 data, and that the data are well explained by a model using oxygen isotope exchange reactions. We propose that the oxygen isotope exchange occurs between APS and cytoplasmic water, and/or between sulfite and adenosine monophosphate (AMP) during APS formation. Model calculations show that cell external reoxidation of reduced sulfur species would require up to 3000 mol/m(3) of an oxidant at ODP Site 1130, which is incompatible with the sediment geochemical data. In addition, we show that the volumetric fluxes required to explain the observed delta O-18(SO4)2- data are on average 14 times higher than the volumetric sulfate reduction rates (SRR) obtained from inverse modeling of the porewater data. The ratio between the gross sulfate flux into the microbes and the net sulfate flux through the microbes is depth invariant, and independent of sulfide concentrations. This suggests that both fluxes are controlled by cell density and that cell-specific sulfate reduction rates remain constant with depth. (C) 2007 Elsevier Ltd. All rights reserved. C1 Univ Toronto, Dept Geol, Geobiol Isotope Lab, Toronto, ON M5S 3B1, Canada. ETH, Inst Geol, CH-8092 Zurich, Switzerland. CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. Leibniz Inst Balt Sea Res, D-18119 Warnemunde, Germany. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. RP Wortmann, UG (reprint author), Univ Toronto, Dept Geol, Geobiol Isotope Lab, 22 Russellstr, Toronto, ON M5S 3B1, Canada. EM uli.wortmann@utoronto.ca RI Brunner, Benjamin/F-2027-2011; Bottcher, Michael /A-6746-2013; Bernasconi, Stefano/E-5394-2010; Swart, Peter/K-7041-2016; OI Bernasconi, Stefano/0000-0001-7672-8856; Wortmann, Ulrich/0000-0001-7854-9173 NR 53 TC 60 Z9 61 U1 3 U2 36 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 SEP 1 PY 2007 VL 71 IS 17 BP 4221 EP 4232 DI 10.1016/j.gca.2007.06.033 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 209CD UT WOS:000249365000007 ER PT J AU Dickey, JO Marcus, SL Chin, TM AF Dickey, Jean O. Marcus, Steven L. Chin, Toshio M. TI Thermal wind forcing and atmospheric angular momentum: Origin of the Earth's delayed response to ENSO SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ROTATION AB Interannual length-of-day variations and ENSO indices such as the Southern Oscillation Index ( SOI) and Nino 3.4 SST are well correlated as a consequence of angular momentum conservation. During an El Nino event, the westerly winds increase, which raises the atmospheric angular momentum ( AAM); as a result, the solid Earth must slow down, which increases the duration of the day ( length-of-day: LOD). However, a lag has been observed with the SOI and Nino 3.4 SST leading the LOD and AAM series by one-two months; to date no dynamical explanation has been offered. The dominant excitation mechanism of interannual LOD is the wind term, driven largely by thermal winds arising from the poleward gradient of tropical temperature ( TT). We show that the TT gradient ( TTG), which peaks 1-2 months after the Nino 3.4 SST anomaly, is the source of the thermal winds that drive the LOD anomaly and account for this well-known ENSO-Earth rotation lag. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dickey, JO (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jean.o.dickey@jpl.nasa.gov OI Marcus, Steven/0000-0002-5763-6961 NR 11 TC 5 Z9 5 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 1 PY 2007 VL 34 IS 17 AR L17803 DI 10.1029/2007GL030846 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 208QR UT WOS:000249334800005 ER PT J AU Hansen, K AF Hansen, Kathryn TI Controversy in the cradle of humankind SO GEOTIMES LA English DT Article C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hansen, K (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 USA SN 0016-8556 J9 GEOTIMES JI Geotimes PD SEP PY 2007 VL 52 IS 9 BP 30 EP 33 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 207FY UT WOS:000249238200027 ER PT J AU Behringer, RP Wilkinson, A Metzger, PT AF Behringer, R. P. (Bob) Wilkinson, Allen Metzger, Philip T. TI Untitled SO GRANULAR MATTER LA English DT Editorial Material C1 Duke Univ, Dept Phys, Durham, NC 27708 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NASA, KSC, Appl Phys Lab, Kennedy Space Ctr, FL 32899 USA. RP Behringer, RP (reprint author), Duke Univ, Dept Phys, Durham, NC 27708 USA. EM bob@phy.duke.edu RI Metzger, Philip/R-3136-2016 OI Metzger, Philip/0000-0002-6871-5358 NR 0 TC 0 Z9 0 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 1434-7636 J9 GRANUL MATTER JI Granul. Matter PD SEP PY 2007 VL 9 IS 5 BP 293 EP 294 DI 10.1007/s10035-007-0048-0 PG 2 WC Materials Science, Multidisciplinary; Mechanics; Physics, Applied SC Materials Science; Mechanics; Physics GA 204BY UT WOS:000249019100001 ER PT J AU Dohm, JM Barlow, NG Anderson, RC Williams, JP Miyamoto, H Ferris, JC Strom, RG Taylor, J Fairen, AG Baker, VR Boynton, WV Keller, JM Kerry, K Janes, D Rodriguez, JAP Hare, TM AF Dohm, James M. Barlow, Nadine G. Anderson, Robert C. Williams, Jean-Pierre Miyamoto, Hirdy Ferris, Justin C. Strom, Robert G. Taylor, Jeffrey Fairen, Alberto G. Baker, Victor R. Boynton, William V. Keller, John M. Kerry, Kris Janes, Daniel Rodriguez, J. A. P. Hare, Trent M. TI Possible ancient giant basin and related water enrichment in the Arabia Terra province, Mars SO ICARUS LA English DT Review DE Mars; geological processes; geophysics; impact processes; tectonics ID PLANETARY WRINKLE RIDGES; ORBITER LASER ALTIMETER; INNER SOLAR-SYSTEM; CRATER EJECTA; GLOBAL DISTRIBUTION; ORIGIN; THARSIS; TOPOGRAPHY; EVOLUTION; ICE AB A circular albedo feature in the Arabia Terra province was first hypothesized as an ancient impact basin using Viking-era information. To test this unpublished hypothesis, we have analyzed the Viking era-information together with layers of new data derived from the Mars Global Surveyor (MGS) and Mars Odyssey (MO) missions. Our analysis indicates that Arabia Terra is an ancient geologic province of Mars with many distinct characteristics, including predominantly Noachian materials, a unique part of the highland-lowland boundary, a prominent paleotectonic history, the largest region of fretted terrain on the planet, outflow channels with no obvious origins, extensive exposures of eroded layered sedimentary deposits, and notable structural, albedo, thermal inertia, gravity, magnetic, and elemental signatures. The province also is marked by special impact crater morphologies, which suggest a persistent volatile-rich substrate. No one characteristic provides definitive answers to the dominant event(s) that shaped this unique province. Collectively the characteristics reported here support the following hypothesized sequence of events in Arabia Terra: (1) an enormous basin, possibly of impact origin, formed early in martian history when the magnetic dynamo was active and the lithosphere was relatively thin, (2) sediments and other materials were deposited in the basin during high erosion rates while maintaining isostatic equilibrium, (3) sediments became water enriched during the Noachian Period, and (4) basin materials were uplifted in response to the growth of the Tharsis Bulge, resulting in differential erosion exposing ancient stratigraphic sequences. Parts of the ancient basin remain water-enriched to the present day. (c) 2007 Elsevier Inc. All rights reserved. C1 Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Tokyo, Univ Museum, Tokyo 1130033, Japan. Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. Natl Ocean & Atmospher Adm, Natl Weather Serv, Palmer, AK 99645 USA. Univ Hawaii, Inst Geophys & Planetol, Honolulu, HI 96822 USA. Univ Autonoma Madrid, CSIC, Ctr Biol Mol, Madrid 28049, Spain. NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. Inst Plant Sci, Tucson, AZ 85719 USA. US Geol Survey, Flagstaff, AZ 86001 USA. RP Dohm, JM (reprint author), Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. EM jmd@hwr.arizona.edu RI Miyamoto, Hideaki/B-9666-2008; Miyamoto, Hideaki/E-3381-2012; Williams, Jean-Pierre/C-3531-2009; Dohm, James/A-3831-2014; OI Williams, Jean-Pierre/0000-0003-4163-2760; Hare, Trent/0000-0001-8842-389X NR 115 TC 27 Z9 27 U1 1 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 SEP PY 2007 VL 190 IS 1 BP 74 EP 92 DI 10.1016/j.icarus.2007.03.006 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204EB UT WOS:000249025300006 ER PT J AU Rappaport, NJ Iess, L Tortora, P Anabtawi, A Asmar, SW Somenzi, L Zingoni, F AF Rappaport, Nicole J. Iess, Luciano Tortora, Paolo Anabtawi, Aseel Asmar, Sarni W. Somenzi, Lucia Zingoni, Francesco TI Mass and interior of Enceladus from Cassini data analysis SO ICARUS LA English DT Article DE Saturn; satellites; interiors ID SATURNIAN SYSTEM; GRAVITY-FIELD; TRACKING DATA; SATELLITES; SPACECRAFT AB Gravity results are available from radio Doppler data acquired by the Deep Space Network during the encounter of the Cassini spacecraft with Enceladus in February 2005. We report the mass of Enceladus to be (1.798 +/- 0.0016) x 10(20) kg, which implies a density of 1608.9 +/- 4 kg m(-3). the core radius is similar to 190 kin and the quadrupole mornent C(22) similar to 1.4 x 10(-3). For a core made of hydrated silicates with a density of 2500 kg m(-3) If Enceladus is in hydrostatic equilibrium, the larger than previously anticipated density implies that the recently proposed secondary spin-orbit resonance cannot be present. Therefore, the Source of endogenic activity of Enceladus remains unexplained. (c) 2007 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Roma La Sapienza, Dipartimento Ingn Aerospaziale Astronaut, I-00184 Rome, Italy. Univ Bologna, DIEM Fac Ingn 2, I-47100 Forli, Italy. RP Rappaport, NJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nicole.j.rappaport@jpl.nasa.gov RI IESS, Luciano/F-4902-2011; Tortora, Paolo/J-6191-2012 OI IESS, Luciano/0000-0002-6230-5825; Tortora, Paolo/0000-0001-9259-7673 NR 24 TC 10 Z9 10 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 J9 ICARUS JI Icarus PD SEP PY 2007 VL 190 IS 1 BP 175 EP 178 DI 10.1016/j.icarus.2007.03.025 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204EB UT WOS:000249025300013 ER PT J AU Castillo-Rogez, JC Matson, DL Sotin, C Johnson, TV Lunine, JI Thomas, PC AF Castillo-Rogez, J. C. Matson, D. L. Sotin, C. Johnson, T. V. Lunine, J. I. Thomas, P. C. TI Iapetus' geophysics: Rotation rate, shape, and equatorial ridge SO ICARUS LA English DT Review DE Iapetus; interiors; geophysics; satellites; shapes; satellites; dynamics ID TEMPERATURE-DEPENDENT VISCOSITY; LARGE ICY SATELLITES; EARLY SOLAR-SYSTEM; THERMAL-CONVECTION; GALILEAN SATELLITES; TIDAL DISSIPATION; NEARBY SUPERNOVA; GIANT PLANETS; EVOLUTION; TOPOGRAPHY AB Iapetus has preserved evidence that constrains the modeling of its geophysical history from the time of its accretion until now. The evidence is (a) its present 79.33-day rotation or spin rate, (b) its shape that corresponds to the equilibrium figure for a hydrostatic body rotating with a period of similar to 16 h, and (c) its high, equatorial ridge, which is unique in the Solar System. This paper reports the results of an investigation into the coupling between Iapetus' thermal and orbital evolution for a wide range of conditions including the spatial distributions with time of composition, porosity. short-lived radioactive isotopes (SLRI), and temperature. The thermal model uses conductive heat transfer with temperature-dependent conductivity. Only models with a thick lithosphere and an interior viscosity in the range of about the water ice melting point can explain the observed shape. Short-lived radioactive isotopes provide the heat needed to decrease porosity in Iapetus' early history. This increases thermal conductivity and allows the development of the strong lithosphere that is required to preserve the 16-h rotational shape and the high vertical relief of the topography. Long-lived radioactive isotopes and SLRI raise internal temperatures high enough that significant tidal dissipation can start, and despin Iapetus to synchronous rotation. This Occurred several hundred million years after Iapetus formed. The models also constrain the time when Iapetus formed because the successful models are critically dependent upon having just the right amount of heat added by SLRI decay in this early period. The amount of heat available from short-lived radioactivity is not a free parameter but is fixed by the time when Iapetus accreted, by the canonical concentration of (26)A], and, to a lesser extent, by the concentration of Fe-60. The needed amount of heat is available only if Iapetus accreted between 2.5 and 5.0 Myr after the formation of the calcium aluminum inclusions as found in meteorites. Models with these features allow us to explain lapetus' present synchronous rotation, its fossil 16-h shape, and the context within which the equatorial ridge arose. (c) 2007 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Lab Planetol & Geodynam Nantes, CNRS UMR 6112, F-44322 Nantes 3, France. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Castillo-Rogez, JC (reprint author), CALTECH, Jet Prop Lab, M-S 230-260,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM julie.c.castillo@jpl.nasa.gov NR 101 TC 78 Z9 78 U1 2 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP PY 2007 VL 190 IS 1 BP 179 EP 202 DI 10.1016/j.icarus.2007.02.018 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204EB UT WOS:000249025300014 ER PT J AU Moore, MH Ferrante, RF Hudson, RL Stone, JN AF Moore, M. H. Ferrante, R. F. Hudson, R. L. Stone, J. N. TI Ammonia-water ice laboratory studies relevant to outer Solar System surfaces SO ICARUS LA English DT Article DE ices; Charon; Trans-Neptunian objects; satellites; surfaces; spectroscopy ID INFRARED-SPECTRA; ION IRRADIATION; PROTON IRRADIATION; CRYSTALLINE WATER; KUIPER-BELT; TRAILING HEMISPHERES; PHASE; SPECTROSCOPY; ENCELADUS; COMETS AB Although water- and ammonia-ices have been observed or postulated as important components of the icy surfaces of planetary satellites ill the outer Solar System, significant gaps exist in our knowledge of the spectra and behavior of such mixtures under astrophysical conditions. To that end, we have completed low-temperature spectroscopic studies (1-20 mu m) of water-ammonia mixtures, with an emphasis on features in the near-IR, a region which is accessible to ground-based observations. The influences of composition, formation temperature, thermal- and radiation-processing, and phase (crystalline or amorphous) of the components were examined. Spectra of both pure NH3 and H2O-NH3 icy mixtures with ratios from 0.7 to 57 were measured at temperatures from 10 to 120 K. Conditions for the formation and thermal stability of the ammonia hernihydrate (2NH(3)center dot H2O) and the ammonia monohydrate (NH3 center dot H2O) have been examined. Band positions of NH3 in different H2O-ices and major band positions of the hydrates were measured. We report spectral shifts that depend on concentration and temperature. The rachation-induced amorphization of the hernihydrate was observed and the radiation destruction of NH3 in H2O-ices was measured. Implications of these results for the formation, stability, and detection of ammonia on outer satellite surfaces are discussed. (c) 2007 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Astrochem Branch, Greenbelt, MD 20771 USA. USN Acad, Dept Chem, Annapolis, MD 21402 USA. Eckerd Coll, Dept Chem, St Petersburg, FL 33733 USA. RP Moore, MH (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Branch, Code 691, Greenbelt, MD 20771 USA. EM marla.h.moore@nasa.gov RI Hudson, Reggie/E-2335-2012 NR 48 TC 54 Z9 54 U1 3 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD SEP PY 2007 VL 190 IS 1 BP 260 EP 273 DI 10.1016/j.icarus.2007.02.020 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204EB UT WOS:000249025300019 ER PT J AU Yang, RQ Hill, CJ Mansour, K Qiu, YM Soibel, A Muller, RE Echternach, PM AF Yang, Rui Q. Hill, Cory J. Mansour, Kamjou Qiu, Yueming Soibel, Alexander Muller, Richard E. Echternach, Pierre M. TI Distributed feedback mid-IR interband cascade lasers at thermoelectric cooler temperatures SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS LA English DT Article DE diode lasers; mid-IR; quantum well lasers; semiconductor superlattices ID CONTINUOUS-WAVE OPERATION; MU-M; METHANE AB Continuous wave (CW) operation of single-mode distributed feedback interband cascade (IC) lasers has been demonstrated at temperatures up to 261 K near similar to 3.3 mu m with sidemode-suppression ratio greater than 20 dB. The electrical power consumption is less than 1.1 W over the entire operating range, which enables CW operation using only thermoelectric cooling from ambient temperatures. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yang, RQ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Rui.Q.Yang@JPL.nasa.gov; Cory.J.Hill@JPL.nasa.gov; Kamjou.Mansour@JPL.nasa.gov; Yueming.Qiu@JPL.nasa.gov; Alexander.Soibel@JPL.nasa.gov; Richard.E.Muller@JPL.nasa.gov; Pierre.M.Echtemach@JPL.nasa.gov RI Soibel, Alexander/A-1313-2007 NR 13 TC 25 Z9 26 U1 2 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1077-260X J9 IEEE J SEL TOP QUANT JI IEEE J. Sel. Top. Quantum Electron. PD SEP-OCT PY 2007 VL 13 IS 5 BP 1074 EP 1078 DI 10.1109/JSTQE.2007.903014 PN 1 PG 5 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 223ME UT WOS:000250373800005 ER PT J AU Wang, CC Trivedi, SB Jin, F Stepanov, S Chen, Z Khurgin, J Rodriguez, P Prasad, NS AF Wang, Chen-Chia Trivedi, Sudhir B. Jin, Feng Stepanov, Serguei Chen, Zhongyang Khurgin, Jacob Rodriguez, Ponciano Prasad, Narasimha S. TI Human life signs detection using high-sensitivity pulsed laser vibrometer SO IEEE SENSORS JOURNAL LA English DT Article DE biomedical acoustics; biomedical measurements; medical diagnosis; optical velocity measurement; photodetectors; vibration measurement AB We demonstrate experimentally the detection, in a remote and noncontact manner, of human life signs using a high-sensitivity pulsed laser vibrometer. The high surface displacement detection sensitivity of the photo-electromotive-force (photo-ENW) pulsed laser vibrometer, combined with its tolerance to the presence and moderate temporal variations of optical speckles in the light beams, allows the detection of human heartbeats, breathing, and gross physical movement from essentially any part of a human subject's surface, even in the presence of clothing, all the while without limiting the interrogation points to specific locations like the chest and carotid areas. In contrast to conventional Michelson interferometer-based laser vibrometers, the photo-EMF pulsed laser vibrometer (PPLV) does not require the use of retroreflective tapes or special electronic filtering to retrieve vividly the biological subject's life signs. Experimental results demonstrating the detection of life signs from various parts of biological subjects' bodies, with or without the coverage of clothing are presented. We also demonstrate the monitoring of a human subject's heart movements by interrogating the back of his/her hand. Results from using PPLV to determine extremity blood circulation at various levels of proximal occluding pressures are also presented. C1 Brimrose Corp, Baltimore, MD 21236 USA. CICISE, Mexico City 22860, DF, Mexico. Johns Hopkins Univ, Dept Elect & Comp Engn, Baltimore, MD 21218 USA. Inst Nacl Astrofis Opt & Electr, Puebla 7200, Mexico. NASA, Langley Res Ctr, Hampton, VA USA. RP Wang, CC (reprint author), Brimrose Corp, Baltimore, MD 21236 USA. EM ccwang@brimrose.com; strivedi@brimrose.com; fjin@brimrose.com; steps@cicese.mx; zychen@brimrose.com; jakek@jhu.edu; ponciano@inaoep.mx; n.s.prasad@larc.nasa.gov RI khurgin, Jacob/A-3278-2010 NR 9 TC 8 Z9 8 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1530-437X J9 IEEE SENS J JI IEEE Sens. J. PD SEP-OCT PY 2007 VL 7 IS 9-10 BP 1370 EP 1376 DI 10.1109/JSEN.2007.905041 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA 214MQ UT WOS:000249742700027 ER PT J AU Teverovsky, A AF Teverovsky, Alexander TI Effect of mechanical stresses on characteristics of chip tantalum capacitors SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY LA English DT Article DE degradation; mechanical stress; tantalum capacitor AB The effect of compressive mechanical stresses on chip solid tantalum capacitors is investigated by monitoring the characteristics of different part types under axial and hydrostatic stresses. An exponential increase of leakage currents was observed when stresses exceeded a critical value, which varied on average from 10 to 40 MPa depending on the part type. For the first time, reversible variations of leakage currents (up to two orders of magnitude) with stress have been demonstrated. Mechanical stresses did not cause significant changes of ac characteristics of the capacitors, whereas breakdown voltages measured during the surge-current testing decreased substantially, indicating an increased probability of failures of stressed capacitors in low-impedance applications. Variations of leakage currents are explained by a combination of two mechanisms: stress-induced scintillations and stress-induced generation of electron traps in the tantalum pentoxide dielectric. C1 Perot Syst NASA, Goddard Space Flight Ctr, Parts Anal Lab, Greenbelt, MD 20771 USA. RP Teverovsky, A (reprint author), Perot Syst NASA, Goddard Space Flight Ctr, Parts Anal Lab, Code 661, Greenbelt, MD 20771 USA. EM Alexander.A.Teverovsky.I@gsfc.nasa.gov NR 20 TC 3 Z9 3 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1530-4388 J9 IEEE T DEVICE MAT RE JI IEEE Trans. Device Mater. Reliab. PD SEP PY 2007 VL 7 IS 3 BP 399 EP 406 DI 10.1109/TDMR.2007.907289 PG 8 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 259BI UT WOS:000252913700002 ER PT J AU Klimeck, G Ahmed, SS Bae, H Kharche, N Rahman, R Clark, S Haley, B Lee, SH Naumov, M Ryu, H Saied, F Prada, M Korkusinski, M Boykin, TB AF Klimeck, Gerhard Ahmed, Shaikh Shahid Bae, Hansang Kharche, Neerav Rahman, Rajib Clark, Steve Haley, Benjamin Lee, Sunhee Naumov, Maxim Ryu, Hoon Saied, Faisal Prada, Marta Korkusinski, Marek Boykin, Timothy B. TI Atomistic simulation of realistically sized nanodevices using NEMO 3-D - Part I: Models and benchmarks SO IEEE TRANSACTIONS ON ELECTRON DEVICES LA English DT Article DE atomistic simulation; Keating model; nanostructures; piezoelectricity; quantum computation; strain; tight binding; valley splitting; 3-D NanoElectronic MOdeling (NEMO 3-D) ID TIGHT-BINDING PARAMETERS; QUANTUM DOTS; ELECTRONIC-STRUCTURE; STRAIN-ENERGY; SEMICONDUCTORS AB Device physics and material science meet at the atomic scale of novel nanostructured semiconductors, and the distinction between new device or new material is blurred. Not only the quantum-mechanical effects in the electronic states of the device but also the granular atomistic representation of the underlying material are important. Approaches based on a continuum representation of the underlying material typically used by device engineers and physicists become invalid. Ab initio methods used by material scientists typically do not represent the band gaps and masses precisely enough for device design, or they do not scale to realistically large device sizes. The plethora of geometry, material, and doping configurations in semiconductor devices at the nanoscale suggests that a general nanoelectronic modeling tool is needed. The 3-D NanoElectronic MOdeling (NEMO 3-D) tool has been developed to address these needs. Based on the atomistic valence force field and a variety of nearest neighbor tight-binding models (e.g., s, sp(3) s*, and sp(3)d(5)s*), NEMO 3-D enables the computation of strain and electronic structure for more than 64 and 52 million atoms, corresponding to volumes of (110 nm)(3) and (101 nm)(3), respectively. The physical problem may involve very large scale computations, and NEW 3-D has been designed and optimized to be scalable from single central processing units to large numbers of processors on commodity clusters and supercomputers. NEMO 3-D has been released with an open-source license in 2003 and is continually developed by the Network for Computational Nanotechnology (NCN). A web-based online interactive version for educational purposes is freely available on the NCN portal (http://www.nanoHUB.org). In this paper, theoretical models and essential algorithmic and computational components that have been used in the development and successful deployment of NEMO 3-D are discussed. C1 Purdue Univ, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA. Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Purdue Univ, Rosen Ctr Adv Comp, W Lafayette, IN 47907 USA. Purdue Univ, Dept Comp Sci, W Lafayette, IN 47907 USA. Natl Res Council Canada, Inst Microstruct Sci, Quantum Theory Grp, Ottawa, ON K1A 0R6, Canada. Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA. RP Klimeck, G (reprint author), Purdue Univ, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA. EM gekco@purdue.edu RI Fonseca, James/G-1018-2011; Kharche, Neerav/F-4331-2015; Klimeck, Gerhard/A-1414-2012; OI Kharche, Neerav/0000-0003-1014-6022; Klimeck, Gerhard/0000-0001-7128-773X; Rahman, Rajib/0000-0003-1649-823X NR 44 TC 124 Z9 124 U1 1 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9383 J9 IEEE T ELECTRON DEV JI IEEE Trans. Electron Devices PD SEP PY 2007 VL 54 IS 9 BP 2079 EP 2089 DI 10.1109/TED.2007.902879 PG 11 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 205HP UT WOS:000249104900002 ER PT J AU Klimeck, G Ahmed, SS Kharche, N Korkusinski, M Usman, M Prada, M Boykin, TB AF Klimeck, Gerhard Ahmed, Shaikh Shahid Kharche, Neerav Korkusinski, Marek Usman, Muhammad Prada, Marta Boykin, Timothy B. TI Atomistic simulation of realistically sized nanodevices using NEMO 3-D - Part II: Applications SO IEEE TRANSACTIONS ON ELECTRON DEVICES LA English DT Article DE atomistic simulation; Keating model; nanostruetures; nanowire; NEMO 3-D; piezoelectricity; quantum computation; quantum dot (QD); quantum well (QW); strain; tight binding; valley splitting (VS) ID QUANTUM; NANOWIRES; LASER; TIME AB In Part 1, the development and deployment of a general nanoelectronic modeling tool (NEMO 3-D) has been discussed. Based on the atomistic valence-force field and the sp(3)d(5)s*. nearest neighbor tight-binding models, NEMO 3-D enables the computation of strain and electronic structure in nanostructures consisting of more than 64 and 52 million atoms, corresponding to volumes of (110 nm)(3) and (101 nm)(3), respectively. In this part, successful applications of NEMO 3-D are demonstrated in the atomistic calculation of single-particle electronic states of the following realistically sized nanostructures: 1) self-assembled quantum dots (QDs) including long-range strain and piezoelectricity; 2) stacked quantum dot system as used in quantum cascade lasers; 3) SiGe quantum wells (QWs) for quantum computation; and 4) SiGe nanowires. These examples demonstrate the broad NEMO 3-D capabilities and indicate the necessity of multimillion atomistic electronic structure modeling. C1 Purdue Univ, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA. Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Natl Res Council Canada, Quantum Theory Grp, Ottawa, ON K1A 0R6, Canada. Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA. RP Klimeck, G (reprint author), Purdue Univ, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA. EM gekco@purdue.edu RI Usman, Muhammad/C-1557-2012; Kharche, Neerav/F-4331-2015; Klimeck, Gerhard/A-1414-2012 OI Kharche, Neerav/0000-0003-1014-6022; Klimeck, Gerhard/0000-0001-7128-773X NR 39 TC 68 Z9 68 U1 2 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9383 J9 IEEE T ELECTRON DEV JI IEEE Trans. Electron Devices PD SEP PY 2007 VL 54 IS 9 BP 2090 EP 2099 DI 10.1109/TED.2007.904877 PG 10 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 205HP UT WOS:000249104900003 ER PT J AU Kanagaratnam, P Markus, T Lytle, V Heavey, B Jansen, P Prescott, G Gogineni, SP AF Kanagaratnam, Pannirselvam Markus, Thorsten Lytle, Victoria Heavey, Brandon Jansen, Peter Prescott, Glenn Gogineni, Siva Prasad TI Ultrawideband radar measurements of thickness of snow over sea ice SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Antarctica; FM-CW radar; microwave; sea ice snow; ultrawideband radar ID MICROWAVE SIGNATURES; VOLUME-SCATTERING; SOUTHERN-OCEAN; MODEL; SURFACE; WAVE AB An accurate knowledge of snow thickness and its variability over sea ice is crucial in determining the overall polar heat and freshwater budget, which influences the global climate. Recently, algorithms have been developed to extract snow thicknesses from satellite passive microwave data. However, validation of these data over the large footprint of the passive microwave sensor has been a challenge. The only method used thus far has been with meter sticks during ship cruises. To address this problem, we developed an ultrawideband frequency-modulated continuous-wave radar to measure the snow thickness over sea ice. We synthesized a very linear chirp signal by using a phase-locked loop with a digitally generated chirp signal as a reference to obtain a fine-range resolution. The radar operates over the frequency range from 2-8 GHz. We made snow-thickness measurements over the Antarctic sea ice by operating the radar from a sled in September and October 2003. We performed radar measurements over 11 stations with varying snow thicknesses between 4 and 85 cm. We observed an excellent agreement between radar estimates of snow thickness with physical measurements, achieving a correlation coefficient of 0.95 and a vertical resolution of about 3 cm. Comparison of simulated radar waveforms using a simple transmission line model with the measurements confirms our expectations that echoes from snow-covered sea ice are dominated by reflections from air-snow and snow-ice interfaces. C1 Climate & Cryosphere Program, N-9296 Tromso, Norway. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Australian Govt Antarctic Div, Kingston, Tas, Australia. Univ Kansas, Dept Elect & Comp Engn, Lawrence, KS 66045 USA. NASA, Goddard Space Flight Ctr, Earth Sci Technol Off, Greenbelt, MD 20771 USA. Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA. RP Kanagaratnam, P (reprint author), Climate & Cryosphere Program, N-9296 Tromso, Norway. RI Markus, Thorsten/D-5365-2012 NR 28 TC 16 Z9 16 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2007 VL 45 IS 9 BP 2715 EP 2724 DI 10.1109/TGRS.2007.900673 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 205HU UT WOS:000249105400003 ER PT J AU Le Vine, DM Jacob, SD Dinnat, EP De Matthaeis, P Abraham, S AF Le Vine, David M. Jacob, S. Daniel Dinnat, Emmanuel P. De Matthaeis, Paolo Abraham, Saji TI The influence of antenna pattern on Faraday rotation in remote sensing at L-band SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE antenna patterns; Faraday rotation; microwave remote sensing; radiometer ID SEA-SURFACE SALINITY; SPACE; POLARIZATION; IONOSPHERE AB The influence of the pattern of the receive antenna on measured Faraday rotation is examined in the context of passive remote sensing of soil moisture and ocean salinity at L-band. Faraday rotation is an important consideration for radiometers on future missions in space, such as SMOS and Aquarius. Using the radiometer on Aquarius as an example, it is shown that, while I = Tv + Th is independent of Faraday rotation to first order, it has rotation dependence when realistic antenna patterns are included in the analysis. In addition, it is shown that using the third Stokes parameter to measure the rotation angle can yield a result that is biased by as much as 1 degrees by purely geometrical issues that are associated with the finite width of the main beam. C1 NASA, Goddard Space Flight Ctr, Lab Hydrospher & Biospher Sci, Instrument Sci Branch, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, RS Informat Syst Inc, Greenbelt, MD 20771 USA. RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Lab Hydrospher & Biospher Sci, Instrument Sci Branch, Greenbelt, MD 20771 USA. RI Dinnat, Emmanuel/D-7064-2012 OI Dinnat, Emmanuel/0000-0001-9003-1182 NR 21 TC 9 Z9 9 U1 1 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2007 VL 45 IS 9 BP 2737 EP 2746 DI 10.1109/TGRS.2007.898237 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 205HU UT WOS:000249105400005 ER PT J AU Sun, JQ Xiong, XX AF Sun, Jun-Qiang Xiong, Xiaoxiong TI MODIS polarization-sensitivity analysis SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Moderate Resolution Imaging Spectroradiometer (MODIS); polarization; reflective solar bands (RSBs) ID IMAGING SPECTRORADIOMETER MODIS; TERRA MODIS; PERFORMANCE; CALIBRATION; WATER; LAND; AQUA AB The Moderate Resolution Imaging Spectroradiometer (MODIS) is one of the primary instruments in the Earth Observing System (EOS). Currently, MODIS instruments are onboard the NASA EOS Terra and Aqua spacecraft launched in December 1999 and May 2002, respectively. The MODIS reflective solar bands (RSBs) are sensitive to the polarization of incident light, particularly for the visible bands. To derive accurate top-of-the-atmosphere radiances, it is essential to know the polarization sensitivity, characterized by a polarization factor and phase angle, of the instruments. From prelaunch polarization sensitivity measurements, the polarization factors and phase angles for all visible and near-infrared bands of both instruments are derived, analyzed, and compared. The polarization factors are wavelength, angle of incidence on the MODIS scan mirror, and detector-dependent. For Terra MODIS, they are also mirrorside-dependent. The 412-nm band has the largest polarization factor, which is about 0.04 for both instruments. The polarization factors of all other bands are either smaller than or close to 0.02, which is the polarization requirement for the MODIS RSB whose wavelengths are longer than 412 nm. The unexpected one-, three-, and four-cycle anomalies observed in the measurements are analyzed. These anomalies are shown to be likely due to the nonuniformity of the light source and the retro-reflected light from the MODIS optical system. Their impacts on the derived polarization parameters are estimated and discussed. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sun, JQ (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NR 23 TC 24 Z9 24 U1 2 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2007 VL 45 IS 9 BP 2875 EP 2885 DI 10.1109/TGRS.2007.900672 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 205HU UT WOS:000249105400016 ER PT J AU Yang, P Zhang, L Hong, G Nasiri, SL Baum, BA Huang, HL King, MD Platnick, S AF Yang, Ping Zhang, Lei Hong, Gang Nasiri, Shaima L. Baum, Bryan A. Huang, Hung-Lung King, Michael D. Platnick, Steven TI Differences between collection 4 and 5 MODIS ice cloud optical/microphysical products and their impact on radiative forcing simulations SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aqua; clouds; Moderate Resolution Imaging Spectroradiometer (MODIS); radiative forcing; remote sensing; static libraries ID SINGLE-SCATTERING PROPERTIES; OPTICAL-THICKNESS; CIRRUS CLOUDS; INFRARED RADIANCES; LIGHT-SCATTERING; TROPICAL CIRRUS; CLIMATE MODELS; PART II; PARAMETERIZATION; CRYSTALS AB This paper reports on the comparison of two latest versions (collections 4 and 5) of ice cloud products derived from the Moderate Resolution Imaging Spectroradiometer (MODIS) measurements. The differences between the bulk optical properties of ice clouds used in collections 4 and 5 and the relevant impact on simulating the correlation of the bidirectional reflection functions at two MODIS bands centered at 0.65 (or 0.86) and 2.13 mu m are investigated. The level-3 MODIS ice cloud properties (specifically, ice cloud fraction, optical thickness, and effective particle size in this paper) from the collection 4 and 5 datasets; are compared for a tropical belt of 30 degrees S-30 degrees N. Furthermore, the impact of the differences between the MODIS collection 4 and 5 ice cloud products on the simulation of the radiative forcing of these clouds is investigated. Over the tropics, the averaged ice cloud fraction from collection 5 is 1. 1% more than the collection 4 counterpart, the averaged optical thickness from collection 5 is 1.2 larger than the collection 4 counterpart, and the averaged effective particle radius from collection 5 is 1.8 mu m smaller than the collection 4 counterpart. Moreover, the magnitude of the differences between collection 5 and 4 ice cloud properties also depends on the surface characteristics, i.e., over land or over ocean. The differences of these two datasets (collections 4 and 5) of cloud properties can have a significant impact on the simulation of the radiative forcing of ice clouds. In terms of total (longwave plus shortwave) cloud radiative forcing, the differences between the collection, 5 and 4 results are distributed primarily between -60 and 20 W . m(-2) but peak at 0 W . m(-2). C1 Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM pyang@ariel.met.tamu.edu RI Yang, Ping/B-4590-2011; Baum, Bryan/B-7670-2011; King, Michael/C-7153-2011; Nasiri, Shaima/C-8044-2011; Hong, Gang/A-2323-2012; Platnick, Steven/J-9982-2014 OI Baum, Bryan/0000-0002-7193-2767; King, Michael/0000-0003-2645-7298; Platnick, Steven/0000-0003-3964-3567 NR 61 TC 39 Z9 39 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2007 VL 45 IS 9 BP 2886 EP 2899 DI 10.1109/TGRS.2007.898276 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 205HU UT WOS:000249105400017 ER PT J AU Liu, QH Huang, HG Qin, WH Fu, KH Li, XW AF Liu, Qinhuo Huang, Huaguo Qin, Wenhan Fu, Kaihua Li, Xiaowen TI An extended 3-D radiosity-graphics combined model for studying thermal-emission directionality of crop canopy SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE component temperature; crop canopy; directional brightness temperature (DBT); radiosity-graphics combined model (RGM); thermal-emission directionality ID RADIATIVE-TRANSFER; NATURAL SURFACES; VEGETATION CANOPIES; ROW CROPS; TEMPERATURE; REFLECTANCE; LIGHT; SCATTERING; SATELLITE; RADIANCE AB Radiosity-Graphics combined Model (RGM) has been proposed to calculate the radiation regime and bidirectional reflectance distribution function of complex 3-D scene, which is limited in visible and near-infrared wavelength (0.3-3 mu m) region. In this paper, RGM is extended to thermal region (named as TRGM) based on thermal-radiosity theory and thermal-emission directionality of vegetation canopy. The TRGM has been implemented on Microsoft Windows platform, and a parameterization scheme for crop canopies is introduced in this paper. It is then evaluated by comparing with two row-crop directional thermal emission models and one thermal radiative-transfer model. Field experiment data has been used to validate the TRGM for row structural wheat and maize canopies. The root mean square error of directional brightness temperature (DBT) is smaller than 1.0 degrees C for the wheat canopy and 0.5 degrees Cfor the maize canopy while the canopy DBTs vary more than 4 degrees C. Model sensitivity analyses have also been conducted to illustrate influences of component temperature distribution, component emissivity, incident atmospheric radiation, and canopy structure on the crop canopy DBT. C1 Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing 100101, Peoples R China. Beijing Normal Univ, Beijing 100101, Peoples R China. State Key Lab Remote Sensing Sci, Beijing 100101, Peoples R China. Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. RP Liu, QH (reprint author), Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing 100101, Peoples R China. EM qhliu@irsa.ac.cn NR 48 TC 22 Z9 31 U1 3 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2007 VL 45 IS 9 BP 2900 EP 2918 DI 10.1109/TGRS.2007.902272 PG 19 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 205HU UT WOS:000249105400018 ER PT J AU Haines, SL Jedlovec, GJ Lazarus, SM AF Haines, Stephanie L. Jedlovec, Gary J. Lazarus, Steven M. TI A MODIS sea surface temperature, composite for regional applications SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aqua; composite; Moderate Resolution Imaging Spectroradiometer (MODIS); remote sensing; satellite applications; sea surface temperature (SST) ID SATELLITE AB Sea surface temperature (SST) is an important input for regional and global weather modeling, but timely high-resolution SST data from either in situ or satellite sources are limited. A regional near-real-time Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) 1-km-resolution SST composite has been developed by the NASA Short-term Prediction and Research Transition (SPoRT) program to provide continuous high-resolution SST fields twice daily for regional weather applications. The SPoRT Aqua MODIS SST composite is intercompared to both half-degree-resolution real-time global (RTG) SST analysis and a 6-km-resolution Geostationary Operational Environmental Satellite 12 (GOES) Imager SST analysis and validated against buoy data for the month of May 2004. The SPoRT MODIS composite provides more accurate and detailed spatial information than the RTG-SST or GOES products during this period. Compared to limited buoy data, the daytime MODIS composites for May 2004 were found to have an average cool bias of -0.09 degrees C, and the nighttime composites an average cool bias of -0.29 degrees C, with both day and night composites having correlation values of approximately 0.90. A comparison of the MODIS SST composite to the more recent and higher resolution 12th-degree RTG-SST analysis and the 20th-degree resolution Operational Sea Surface Temperature and Sea Ice Analysis indicated that the SPoRT MODIS composite provides additional spatial and diurnal cycle information on a regional scale. C1 Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. Florida Inst Technol, Melbourne, FL 32901 USA. RP Haines, SL (reprint author), Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35805 USA. EM stephanie.haines@nasa.gov OI Lazarus, Steven/0000-0002-5918-1059 NR 24 TC 28 Z9 28 U1 1 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2007 VL 45 IS 9 BP 2919 EP 2927 DI 10.1109/FGRS.2007.898274 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 205HU UT WOS:000249105400019 ER PT J AU Vorperian, V AF Vorperian, Vatche TI Synthesis of medium voltage dc-to-dc converters from low-voltage, high-frequency PWM switching converters SO IEEE TRANSACTIONS ON POWER ELECTRONICS LA English DT Article DE Dc circuit breaker; feedback control; high-frequency; medium voltage; Neptune power; PWM conversion; reduced average model; redundancy; stacking; reduced real-time model ID POWER-SYSTEM AB Low-voltage dc-to-dc power conversion is a very mature industry which uses high-frequency pulsewidth modulation (PWM) switching techniques. The passive and active components needed to build low-voltage dc-to-dc converters are highly available, affordable and constantly improving. In this paper, a very simple and systematic method of using a large number of lowvoltage, high-frequency PWM converters to synthesize highly redundant, medium voltage (4-40 kV) dc-to-dc converters is presented. Theoretical and practical considerations are discussed in necessary detail and test results of an actual 10-kW, 10 kV-to-400 V, converter built from 48 low-voltage forward converters are presented. Real-time and average reduced circuit models are derived to predict the dynamical behavior of the converter and to design the feedback control loop. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. RP Vorperian, V (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. EM vatche.vorperian@jpl.nasa.gov NR 22 TC 27 Z9 29 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-8993 J9 IEEE T POWER ELECTR JI IEEE Trans. Power Electron. PD SEP PY 2007 VL 22 IS 5 BP 1619 EP 1635 DI 10.1109/TPEL.2007.904170 PG 17 WC Engineering, Electrical & Electronic SC Engineering GA 210HQ UT WOS:000249447700006 ER PT J AU Chen, CLP Guo, TH AF Chen, C. L. Philip Guo, Ten-Huei TI Design of intelligent acceleration schedules for extending the life of aircraft engines SO IEEE TRANSACTIONS ON SYSTEMS MAN AND CYBERNETICS PART C-APPLICATIONS AND REVIEWS LA English DT Article ID FUSION AB Aircraft engine controllers are designed and operated to provide desired performance and stability margins. This paper addresses the relationship between acceleration action and engine component life usage. Based upon this relationship, an intelligent approach for designing acceleration schedules that provide proper tradeoffs between performance and engine life usage is proposed. The benefit of this approach is that it is expected to maintain safety while minimizing the overall operating costs. With the advances of computer technology, engine operation models, and damage physics, it is necessary to reevaluate the control strategy for overall operating cost consideration. This paper uses the thermal-mechanical fatigue (TMF) of a critical component to demonstrate how an intelligent acceleration algorithm can drastically reduce the engine life usage with minimum sacrifice in performance. We have modeled and calculated the probability of failure due to TMF damage. A Monte Carlo simulation is also performed to evaluate the likelihood of engine damage accumulation under various operating conditions. By means of genetic search algorithms, optimal acceleration schedules can be obtained with multiple constraints. The simulation results show that a selected best acceleration schedule can provide a significant life saving in selected engine components. C1 Univ Texas San Antonio, Dept Elect & Comp Engn, San Antonio, TX 78249 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Chen, CLP (reprint author), Univ Texas San Antonio, Dept Elect & Comp Engn, San Antonio, TX 78249 USA. EM philip.chen@utsa.edu; ioguo@grc.nasa.gov RI Chen, C. L. Philip/O-2657-2016 OI Chen, C. L. Philip/0000-0001-5451-7230 NR 21 TC 4 Z9 5 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1094-6977 J9 IEEE T SYST MAN CY C JI IEEE Trans. Syst. Man Cybern. Part C-Appl. Rev. PD SEP PY 2007 VL 37 IS 5 BP 1005 EP 1015 DI 10.1109/TMSCC.2007.902823 PG 11 WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics; Computer Science, Interdisciplinary Applications SC Computer Science GA 204DL UT WOS:000249023700024 ER PT J AU Johnson, A Willson, R Cheng, Y Goguen, J Leger, C Sanmartin, M Matthies, L AF Johnson, Andrew Willson, Reg Cheng, Yang Goguen, Jay Leger, Chris Sanmartin, Miguel Matthies, Larry TI Design through operation of an image-based velocity estimation system for mars landing SO INTERNATIONAL JOURNAL OF COMPUTER VISION LA English DT Article DE velocity estimation; feature tracking; computer vision; robotics; Mars lander; Mars Exploration Rover; DIMES ID AUTONOMOUS HELICOPTER; MOTION AB During the Mars Exploration Rover (MER) landings, the Descent Image Motion Estimation System (DIMES) was used for horizontal velocity estimation. The DIMES algorithm combined measurements from a descent camera, a radar altimeter, and an inertial measurement unit. To deal with large changes in scale and orientation between descent images, the algorithm used altitude and attitude measurements to rectify images to a level ground plane. Feature selection and tracking were employed in the rectified images to compute the horizontal motion between images. Differences of consecutive motion estimates were then compared to inertial measurements to verify correct feature tracking. DIMES combined sensor data from multiple sources in a novel way to create a low-cost, robust, and computationally efficient velocity estimation solution, and DIMES was the first robotics vision system used to control a spacecraft during planetary landing. This paper presents the design and implementation of the DIMES algorithm, the assessment of the algorithm performance using a high fidelity Monte Carlo simulation, validation of performance using field test data and the detailed results from the two landings on Mars. DIMES was used successfully during both MER landings. In the case of Spirit, had DIMES not been used onboard, the total velocity would have been at the limits of the airbag capability. Fortunately, DIMES computed the actual steady state horizontal velocity and it was used by the thruster firing logic to reduce the total velocity prior to landing. For Opportunity. DIMES computed the correct velocity, and the velocity was small enough that the lander performed no action to remove it. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Johnson, A (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 30 TC 17 Z9 23 U1 1 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0920-5691 EI 1573-1405 J9 INT J COMPUT VISION JI Int. J. Comput. Vis. PD SEP PY 2007 VL 74 IS 3 BP 319 EP 341 DI 10.1007/s11263-006-0022-z PG 23 WC Computer Science, Artificial Intelligence SC Computer Science GA 192YG UT WOS:000248239400007 ER PT J AU Zhang, H Mudawar, I Hasan, MM AF Zhang, Hui Mudawar, Issam Hasan, Mohammad M. TI CHF model for subcooled flow boiling in Earth gravity and microgravity SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article ID CRITICAL HEAT-FLUX; TRIGGER MECHANISM; ROUND TUBES; PREDICTION; ORIENTATION; WALL; QUALITIES; LENGTH; LONG AB This study is the first attempt at extending the interfacial Lift-off CHF Model to subcooled flow boiling conditions. A new CHF database was generated for FC-72 from ground tests as well as from microgravity tests that were performed in parabolic flight trajectory. These tests also included high-speed video imaging and analysis of the liquid-vapor interface during the CHF transient. Both the CHF data and the video records played a vital role in constructing and validating the extended CHF model. The fundamental difference between the original Interfacial Lift-off Model, which was developed for saturated flow boiling, and the newly extended model is the partitioning of wall energy between sensible and latent heat for subcooled flow boiling. This partitioning is modeled with the aid of new "heat utility ratio". Using this ratio, the extended Interfacial Lift-off Model is shown to effectively predict both saturated and sub-cooled flow boiling CHF in Earth gravity and in microgravity. (C) 2007 Published by Elsevier Ltd. C1 Purdue Univ, Sch Mech Engn, Boiling & Two Phase Flow Lab, W Lafayette, IN 47907 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mudawar, I (reprint author), Purdue Univ, Sch Mech Engn, Boiling & Two Phase Flow Lab, 585 Purdue Mall, W Lafayette, IN 47907 USA. EM mudawar@ecn.purdue.edu NR 32 TC 14 Z9 14 U1 0 U2 18 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 SEP PY 2007 VL 50 IS 19-20 BP 4039 EP 4051 DI 10.1016/j.ijheatmasstransfer.2007.01.029 PG 13 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 186AF UT WOS:000247750800032 ER PT J AU Kepner, J Zima, H AF Kepner, Jeremy Zima, Hans TI Special issue on high productivity programming languages and models - Preface SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Editorial Material C1 MIT, Lincoln Lab, Lexington, MA 02420 USA. Univ Vienna, A-1010 Vienna, Austria. JPL, Pasadena, CA USA. RP Kepner, J (reprint author), MIT, Lincoln Lab, Lexington, MA 02420 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD FAL PY 2007 VL 21 IS 3 BP 249 EP 250 DI 10.1177/1094342007078434 PG 2 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 202FH UT WOS:000248886900001 ER PT J AU Chamberlain, BL Callahan, D Zima, HP AF Chamberlain, B. L. Callahan, D. Zima, H. P. TI Parallel programmability and the Chapel language SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE parallel languages; productivity; parallel programming; programming models; Chapel AB In this paper we consider productivity challenges for parallel programmers and explore ways that parallel language design might help improve end-user productivity. We offer a candidate list of desirable qualities for a parallel programming language, and describe how these qualities are addressed in the design of the Chapel language. In doing so, we provide an overview of Chapel's features an how they help address parallel productivity. We also survey current techniques for parallel programming and describe ways in which we consider them to fall short of our idealized productive programming model. C1 Cray Res Inc, Seattle, WA 98104 USA. Microsoft Corp, Redmond, WA 98052 USA. Univ Vienna, A-1010 Vienna, Austria. JPL, Pasadena, CA USA. RP Chamberlain, BL (reprint author), Cray Res Inc, Seattle, WA 98104 USA. EM BRADC@CRAY.COM NR 55 TC 194 Z9 195 U1 0 U2 2 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 EI 1741-2846 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD FAL PY 2007 VL 21 IS 3 BP 291 EP 312 DI 10.1177/1094342007078442 PG 22 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 202FH UT WOS:000248886900004 ER PT J AU Diaconescu, RE Zima, HP AF Diaconescu, R. E. Zima, H. P. TI An approach to data distributions in Chapel SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE high productivity language; chapel; user-defined data distributions; locality ID HIGH-PERFORMANCE FORTRAN AB A key characteristic of today's high performance computing systems is a physically distributed memory, which makes the efficient management of locality essential for taking advantage of the performance enhancements offered by these architectures. Currently, the standard technique for programming such systems involves the extension of traditional sequential programming languages with explicit message-passing libraries, in a processor-centric model for programming and execution. It is commonly understood that this programming paradigm results in complex, brittle, and error-prone programs, because of the way in which algorithms and communication are inextricably interwoven. This paper describes a new approach to locality awareness, which focuses on data distributions in high-productivity languages. Data distributions provide an abstract specification of the partitioning of large-scale data collections across memory units, supporting coarse-grain parallel computation and locality of access at a high level of abstraction. Our design, which is based on a new programming language called Chapel, is motivated by the need to provide a high-productivity paradigm for the development of efficient and reusable parallel code. We present an object-oriented framework that allows the explicit specification of the mapping of elements in a collection to memory units, the control of the arrangement of elements within such units, the definition of sequential and parallel iteration over collections, and the formulation of specialized allocation policies as required for advanced applications. The result is a concise high-productivity programming model that separates algorithms from data representation and enables reuse of distributions, allocation policies, and data structures. C1 CALTECH, CACR, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Vienna, Inst Comp Sci, A-1010 Vienna, Austria. RP Diaconescu, RE (reprint author), CALTECH, CACR, Pasadena, CA 91125 USA. EM ZIMA@JPL.NASA.GOV NR 47 TC 10 Z9 10 U1 0 U2 1 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 EI 1741-2846 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD FAL PY 2007 VL 21 IS 3 BP 313 EP 335 DI 10.1177/1094342007078451 PG 23 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 202FH UT WOS:000248886900005 ER PT J AU Lyle, KH Stockwell, AE Hardy, RC AF Lyle, Karen H. Stockwell, Alan E. Hardy, Robin C. TI Application of probability methods to assess airframe crash modeling uncertainty SO JOURNAL OF AIRCRAFT LA English DT Article AB Full-scale aircraft crash simulations. performed with nonlinear, transient dynamic, finite element codes can incorporate structural complexities such as geometrically accurate models, human occupant models, and advanced material models to include nonlinear stress-strain behaviors and. material failure. Validation of these crash simulations is difficult due to a lack of sufficient information to adequately determine the uncertainty in the experimental data and the appropriateness of modeling assumptions. This paper evaluates probabilistic approaches to quantify the effects of finite element modeling assumptions on the predicted responses. The application of probabilistic analysis using finite element simulations of a fuselage vertical drop is the focus of this paper. The results indicate that probabilistic methods show promise for future applications. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Lockheed Martin Mission Serv, Hampton, VA 23681 USA. RP Lyle, KH (reprint author), NASA, Langley Res Ctr, Mail Stop 495, Hampton, VA 23681 USA. NR 13 TC 8 Z9 8 U1 1 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2007 VL 44 IS 5 BP 1568 EP 1573 DI 10.2514/1.27722 PG 6 WC Engineering, Aerospace SC Engineering GA 223IK UT WOS:000250363300015 ER PT J AU Duraisamy, K McCroskey, WJ Baeder, JD AF Duraisamy, Karthikeyan McCroskey, William J. Baeder, James D. TI Analysis of wind tunnel wall interference effects on subsonic unsteady airfoil flows SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 24th Applied Aerodynamics Conference CY JUN 05-08, 2006 CL San Francisco, CA SP Amer Inst Aeronaut & Astronaut ID DIFFERENCE; SCHEMES AB In this work, the effect of wall interference on steady and oscillating airfoils in a subsonic wind tunnel is studied. A variety of approaches including linear theory, compressible inviscid and viscous computations, and experimental data are considered. Integral transform solutions of the linearized potential equations show an augmentation of the lift magnitude for steady flows when the wall is close to the airfoil surface. For oscillating airfoils, lift augmentation is accompanied by a significant change in the phase of the lift response. Idealized compressible Euler calculations are seen to corroborate the linear theory under conditions that are sufficiently away from acoustic resonance. Further, the theory compares well with compressible Reynolds-averaged Navier-Stokes calculations and experimental measurements over a wide range of attached flows at subsonic Mach numbers. The present methodology can thus be used to predict wall interference effects and also to help extrapolate linear and nonlinear (dynamic stall) wind tunnel data to free-air conditions. C1 Univ Maryland, College Pk, MD 20742 USA. NASA, Ames Res Ctr, USA, Aerofightdynam Directorate, Moffett Field, CA 94035 USA. RP Duraisamy, K (reprint author), Univ Glasgow, Dept Engn, Glasgow G12 8QQ, Lanark, Scotland. RI Duraisamy, Karthikeyan/F-2174-2010 NR 14 TC 6 Z9 6 U1 0 U2 7 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2007 VL 44 IS 5 BP 1683 EP 1690 DI 10.2514/1.28143 PG 8 WC Engineering, Aerospace SC Engineering GA 223IK UT WOS:000250363300026 ER PT J AU Mach, DM Koshak, WJ AF Mach, D. M. Koshak, W. J. TI General matrix inversion technique for the calibration of electric field sensor arrays on aircraft platforms SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID THUNDERSTORMS AB A matrix calibration procedure has been developed that uniquely relates the electric fields measured at the aircraft with the external vector electric field and net aircraft charge. The calibration method can be generalized to any reasonable combination of electric field measurements and aircraft. A calibration matrix is determined for each aircraft that represents the individual instrument responses to the external electric field. The aircraft geometry and configuration of field mills (FMs) uniquely define the matrix. The matrix can then be inverted to determine the external electric field and net aircraft charge from the FM outputs. A distinct advantage of the method is that if one or more FMs need to be eliminated or deemphasized ( e. g., due to a malfunction), it is a simple matter to reinvert the matrix without the malfunctioning FMs. To demonstrate the calibration technique, data are presented from several aircraft programs (ER-2, DC-8, Altus, and Citation). C1 UAH, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Mach, DM (reprint author), UAH, Robert Cramer Res Hall,320 Sparkman Dr,Room 4001, Huntsville, AL 35805 USA. EM dmach@nasa.gov NR 17 TC 8 Z9 11 U1 0 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD SEP PY 2007 VL 24 IS 9 BP 1576 EP 1587 DI 10.1175/JTECH2080.1 PG 12 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 215MB UT WOS:000249811500004 ER PT J AU Elliott, HA Jahn, JM Pollock, CJ Moore, TE Horwitz, JL AF Elliott, H. A. Jahn, J-M. Pollock, C. J. Moore, T. E. Horwitz, J. L. TI O+ transport across the polar cap SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE ion osphere/magnetosphere interactions; plasma motion; plasma convection; polar cap phenomena; inner magnetosphere ID INTERPLANETARY MAGNETIC-FIELD; PLASMA SOURCE INSTRUMENT; ION DYNAMICS EXPERIMENT; HIGH-LATITUDE; CENTRIFUGAL ACCELERATION; MAGNETOSPHERIC ELECTRONS; TOPSIDE IONOSPHERE; WIND; OUTFLOW; SIMULATION AB The plasma sheet, inner magnetosphere, and high-latitude magnetosphere all contain significant amounts of O+ ions during active times. Singly charged oxygen ions unambiguously come from the ionosphere, making them an excellent tracer species. We test the cleft ion fountain theory, which asserts that O+ ions escape from the cleft, cross the polar cap, and then enter the plasma sheet. Statistical studies of O+ density in the cleft, high-altitude polar cap, and plasma sheet all indicate that the O+ density increases with increasing solar wind dynamic pressure. In order to examine O+ transport more directly, we use polar cap ion outflow measurements and the 2001 Tsyganenko magnetic field model driven with advanced composition explorer (ACE) solar wind parameters. We calculate the distance between the cleft and the ionospheric footpoints of magnetic field lines mapped from the polar spacecraft along the noon-midnight meridian. Using the observed outflow speed and the magnetic field line length we calculate the travel time for the ions. When we examine the distance from the cleft versus the O+ travel time for individual passes, the slope of the line is consistent with the measured ionospheric convection speed across the polar cap. We conclude that O+ ions emanating principally from the cleft are transported across the polar cap, and these O+ ions have access to the ring current and plasma sheet. (c) 2007 Elsevier Ltd. All rights reserved. C1 SW Res Inst, San Antonio, TX USA. Goddard Space Flight Ctr, Greenbelt, MD USA. Univ Texas, Arlington, TX 76019 USA. RP Elliott, HA (reprint author), SW Res Inst, San Antonio, TX USA. EM helliott@swri.edu RI Moore, Thomas/D-4675-2012 OI Moore, Thomas/0000-0002-3150-1137 NR 45 TC 4 Z9 4 U1 0 U2 1 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 SEP PY 2007 VL 69 IS 13 BP 1541 EP 1555 DI 10.1016/j.jastp.2007.06.003 PG 15 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 215MA UT WOS:000249811300005 ER PT J AU Kondo, H Mojarrab, R Wang, A Phillips, J Almeida, EAC Loftus, DJ Morey-Holton, E Globus, RK Vercoutere, W Limoli, C Searby, ND AF Kondo, H. Mojarrab, R. Wang, A. Phillips, J. Almeida, E. A. C. Loftus, D. J. Morey-Holton, E. Globus, R. K. Vercoutere, W. Limoli, C. Searby, N. D. TI Increased active osteoclasts are associated with acute cancellous bone loss in adult mice exposed to ionizing radiation and musculoskeletal disuse SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Meeting Abstract CT 29th Annual Meeting of the American-Society-for-Bone-and-Mineral-Research CY SEP 16-19, 2007 CL Honolulu, HI SP Amer Soc Bone & Mineral Res C1 [Kondo, H.; Mojarrab, R.; Wang, A.; Phillips, J.; Almeida, E. A. C.; Loftus, D. J.; Morey-Holton, E.; Globus, R. K.; Vercoutere, W.; Searby, N. D.] NASA, Ames Res Ctr, Bone & Signaling Lab, Moffett Field, CA USA. [Limoli, C.] Univ Calif Irvine, Irvine, CA USA. RI Wang, Angela/B-9944-2008 NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER SOC BONE & MINERAL RES PI WASHINGTON PA 2025 M ST, N W, STE 800, WASHINGTON, DC 20036-3309 USA SN 0884-0431 J9 J BONE MINER RES JI J. Bone Miner. Res. PD SEP PY 2007 VL 22 SU 1 BP S217 EP S217 PG 1 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 225IA UT WOS:000250509101171 ER PT J AU Muir, JW Xia, Y Holguin, N Judex, S Qin, Y Evans, H Lang, T Rubin, C AF Muir, J. W. Xia, Y. Holguin, N. Judex, S. Qin, Y. Evans, H. Lang, T. Rubin, C. TI Low magnitude mechanical signals reduce risk-factors for fracture during 90-day bed rest SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Meeting Abstract CT 29th Annual Meeting of the American-Society-for-Bone-and-Mineral-Research CY SEP 16-19, 2007 CL Honolulu, HI SP Amer Soc Bone & Mineral Res C1 [Muir, J. W.; Xia, Y.; Holguin, N.; Judex, S.; Qin, Y.; Rubin, C.] SUNY Stony Brook, Stony Brook, NY USA. [Evans, H.] NASA, Johnson Space Ctr, Houston, TX USA. [Lang, T.] Univ Calif San Francisco, Dept Radiol, San Francisco, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC BONE & MINERAL RES PI WASHINGTON PA 2025 M ST, N W, STE 800, WASHINGTON, DC 20036-3309 USA SN 0884-0431 J9 J BONE MINER RES JI J. Bone Miner. Res. PD SEP PY 2007 VL 22 SU 1 MA T426 BP S338 EP S338 PG 1 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 225IA UT WOS:000250509101646 ER PT J AU Wei, Y Seevaratnam, GK Garoff, S Rame, E Walker, LM AF Wei, Y. Seevaratnam, G. K. Garoff, S. Rame, E. Walker, L. M. TI Dynamic wetting of Boger fluids SO JOURNAL OF COLLOID AND INTERFACE SCIENCE LA English DT Article DE wetting; contact angle; Boger fluid; elastic fluid; non-Newtonian; polymer solution ID MOVING CONTACT LINE; FREE-SURFACE FLOWS; HYDRODYNAMICS; BEHAVIOR; LIQUIDS; ANGLES AB The impact of fluid elasticity on the dynamic wetting of polymer solutions is important because many polymer solutions in technological use exhibit non-Newtonian behaviors in the high shear environment of the wedge-like flow near a moving contact line. Our former study [G.K. Seevaratnam, Y. Suo, E. Rame, L.M. Walker, Phys. Fluids 19 (2007) Art. No. 012103] showed that shear thinning induced by a semi-flexible high molecular weight polymer reduces the viscous bending near a moving contact line as compared to a Newtonian fluid having the same zero-shear viscosity. This results in a dramatic reduction of the dependence of the effective dynamic contact angle on contact line speed. In this paper, we discuss dynamic wetting of Boger fluids which exhibit elasticity-dominated theology with minimal shear thinning. These fluids are prepared by dissolving a dilute concentration of high molecular weight polymer in a "solvent" of the oligomer of the polymer. We demonstrate that elasticity in these fluids increases curvature near the contact line but that the enhancement arises mostly from the weakly non-Newtonian behavior already present in the oligomeric solvent. We present evidence of instabilities on the liquid/vapor interface near the moving contact line. (c) 2007 Elsevier Inc. All rights reserved. C1 Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Carnegie Mellon Univ, Ctr Complex Fluids Engn, Pittsburgh, PA 15213 USA. Carnegie Mellon Univ, Dept Chem Engn, Pittsburgh, PA 15213 USA. NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. RP Garoff, S (reprint author), Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. EM sg2e@andrew.cmu.edu RI Wei, Yuli/A-2814-2012; Garoff, Stephen/P-7629-2014; Walker, Lynn/I-2562-2016 OI Garoff, Stephen/0000-0001-8148-8535; Walker, Lynn/0000-0002-7478-9759 NR 22 TC 10 Z9 10 U1 2 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9797 J9 J COLLOID INTERF SCI JI J. Colloid Interface Sci. PD SEP 1 PY 2007 VL 313 IS 1 BP 274 EP 280 DI 10.1016/j.jcis.2007.04.020 PG 7 WC Chemistry, Physical SC Chemistry GA 194NU UT WOS:000248351900035 PM 17499759 ER PT J AU Cabrol, NA Wettergreen, D Warren-Rhodes, K Grin, EA Moersch, J Diaz, GC Cockell, CS Coppin, P Demergasso, C Dohm, JM Ernst, L Fisher, G Glasgow, J Hardgrove, C Hock, AN Jonak, D Marinangeli, L Minkley, E Ori, GG Piatek, J Pudenz, E Smith, T Stubbs, K Thomas, G Thompson, D Waggoner, A Wagner, M Weinstein, S Wyatt, M AF Cabrol, Nathalie A. Wettergreen, David Warren-Rhodes, Kim Grin, Edmond A. Moersch, Jeffrey Diaz, Guillermo Chong Cockell, Charles S. Coppin, Peter Demergasso, Cecilia Dohm, James M. Ernst, Lauren Fisher, Gregory Glasgow, Justin Hardgrove, Craig Hock, Andrew N. Jonak, Dominic Marinangeli, Lucia Minkley, Edwin Ori, Gian Gabriele Piatek, Jennifer Pudenz, Erin Smith, Trey Stubbs, Kristen Thomas, Geb Thompson, David Waggoner, Alan Wagner, Michael Weinstein, Shmuel Wyatt, Michael TI Life in the Atacama: Searching for life with rovers (science overview) SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID MARSOKHOD FIELD-TEST; GUSEV CRATER; INFRARED-SPECTROSCOPY; MISSION SIMULATION; MICROSCOPIC IMAGER; MERIDIANI-PLANUM; NORTHERN CHILE; SILVER LAKE; MARS; DESERT AB The Life in the Atacama project investigated the regional distribution of life and habitats in the Atacama Desert of Chile. We sought to create biogeologic maps through survey traverses across the desert using a rover carrying biologic and geologic instruments. Elements of our science approach were to: Perform ecological transects from the relatively wet coastal range to the arid core of the desert; use converging evidence from science instruments to reach conclusions about microbial abundance; and develop and test exploration strategies adapted to the search of scattered surface and shallow subsurface microbial oases. Understanding the ability of science teams to detect and characterize microbial life signatures remotely using a rover became central to the project. Traverses were accomplished using an autonomous rover in a method that is technologically relevant to Mars exploration. We present an overview of the results of the 2003, 2004, and 2005 field investigations. They include: The confirmed identification of microbial habitats in daylight by detecting fluorescence signals from chlorophyll and dye probes; the characterization of geology by imaging and spectral measurement; the mapping of life along transects; the characterization of environmental conditions; the development of mapping techniques including homogeneous biological scoring and predictive models of habitat location; the development of exploration strategies adapted to the search for life with an autonomous rover capable of up to 10 km of daily traverse; and the autonomous detection of life by the rover as it interprets observations on-the-fly and decides which targets to pursue with further analysis. C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. Univ Catolica Norte, Antofagasta, Chile. Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Carnegie Mellon Univ, Dept Biol, Pittsburgh, PA 15213 USA. Univ Iowa, Dept Ind Engn, Iowa City, IA 52242 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. Int Res Sch Planetary Sci, I-65127 Pescara, Italy. SETI Inst, Mountain View, CA USA. RP Cabrol, NA (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM ncabrol@mail.arc.nasa.gov RI Moersch, Jeffrey/F-7189-2010; Hardgrove, Craig/C-7333-2011; Dohm, James/A-3831-2014; OI ORI, Gian Gabriele/0000-0002-6460-1476; Demergasso, Cecilia/0000-0003-4563-3066 NR 67 TC 24 Z9 24 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD SEP 1 PY 2007 VL 112 IS G4 AR G04S02 DI 10.1029/2006JG000298 PG 25 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 208RJ UT WOS:000249336600001 ER PT J AU Acikmese, B Ploen, SR AF Acikmese, Behcet Ploen, Scott R. TI Convex programming approach to powered descent guidance for Mars landing SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation and Control Conference CY AUG 15-18, 2005 CL San Francisco, CA SP AIAA ID TRAJECTORY OPTIMIZATION; SEMIDEFINITE AB We present a convex programming algorithm for the numerical solution of the minimum fuel powered descent guidance problem associated with Mars pinpoint landing. Our main contribution is the formulation of the trajectory optimization problem, which has nonconvex control constraints, as a finite-dimensional convex optimization problem, specifically as a second-order cone programming problem. Second-order cone programming is a subclass of convex programming, and there are efficient second-order cone programming solvers with deterministic convergence properties. Consequently, the resulting guidance algorithm can potentially be implemented onboard a spacecraft for real-time applications. C1 CALTECH, Jet Propuls Lab, Guidance & Control Anal Grp, Pasadena, CA 91109 USA. RP Acikmese, B (reprint author), CALTECH, Jet Propuls Lab, Guidance & Control Anal Grp, Mail Stop 198-326, Pasadena, CA 91109 USA. EM Behcet.Acikmese@jpl.nasa.gov; Scott.R.Ploen@jpl.nasa.gov NR 28 TC 63 Z9 68 U1 0 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD SEP-OCT PY 2007 VL 30 IS 5 BP 1353 EP 1366 DI 10.2514/1.27553 PG 14 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 213XQ UT WOS:000249701000014 ER PT J AU Kulkarni, NV Phan, MQ AF Kulkarni, Nilesh V. Phan, Minh Q. TI Neural optimal magnetohydrodynamic control of hypersonic flows SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation and Control Conference CY AUG 11-14, 2003 CL Austin, TX SP Amer Inst Aeronaut & Astronaut ID SYSTEMS C1 Dartmouth Coll, Thayer Sch Engn, Hanover, NH 03755 USA. Perot Syst Inc, Moffett Field, CA 94035 USA. RP Kulkarni, NV (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM nilesh@email.arc.nasa.gov; Minh.Q.Phan@dartmouth.edu NR 12 TC 0 Z9 0 U1 1 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD SEP-OCT PY 2007 VL 30 IS 5 BP 1519 EP 1523 DI 10.2514/1.26315 PG 5 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 213XQ UT WOS:000249701000030 ER PT J AU Mwale, D Gan, TY Shen, SSP Shu, TT Kim, KM AF Mwale, Davison Gan, Thian Yew Shen, Samuel S. P. Shu, Ting Ting Kim, Kyu-Myong TI Wavelet empirical orthogonal functions of space-time-frequency regimes and predictability of southern Africa summer rainfall SO JOURNAL OF HYDROLOGIC ENGINEERING LA English DT Article ID SEA-SURFACE TEMPERATURE; SEASONAL RAINFALL; VARIABILITY; FORECASTS; NAMIBIA AB Wavelet-based empirical orthogonal function (WEOF) analysis was used to analyze the nonstationary spatial, temporal, and frequency regimes of the regional variability in southern African summer (October-March) rainfall. The leading modes of rainfall variability were then used to establish associations with gridded scale-averaged wavelet power of the sea surface temperature (SST) for the Indian and Atlantic Oceans. The WEOF revealed that southern African rainfall is out of phase between areas north and south of 25 degrees S and that areas north of 25 degrees S and northern South Africa experienced decreased rainfall between 1970 and 1997. The decrease in rainfall was modulated by periods of between 2 and 8 years. Using judiciously selected windows of April-May-June SST data for the Atlantic and Indian Oceans as predictors in the artificial neural network-genetic algorithm (ANN-GA), high prediction skill of standardized summer rainfall of southern Africa was achieved. For the validation period 1988-97, Pearson correlation between 0.83 and 0.98 (i.e., 69-96% of observed rainfall variability), Hanssen Kuipers skill scores of between 0.2 and 1.0, and root-mean-square errors of between 0.25 and 0.72 turn of standardized rainfall were found between observed and predicted summer rainfall at a 3-month lead time. C1 Univ Alberta, Dept Civil & Environm Engn, Markin 3033 CNRL, Natl Resources Engn Fac, Edmonton, AB T6G 2W2, Canada. San Diego State Univ, Dept Math & Stat, San Diego, CA 92182 USA. Univ Alberta, Dept Math & Stat Sci, Edmonton, AB T6G 2G7, Canada. NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. RP Gan, TY (reprint author), Univ Alberta, Dept Civil & Environm Engn, Markin 3033 CNRL, Natl Resources Engn Fac, Edmonton, AB T6G 2W2, Canada. EM TGan@ualberta.ca RI Kim, Kyu-Myong/G-5398-2014 NR 24 TC 7 Z9 7 U1 0 U2 1 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 1084-0699 J9 J HYDROL ENG JI J. Hydrol. Eng. PD SEP-OCT PY 2007 VL 12 IS 5 BP 513 EP 523 DI 10.1061/(ASCE)1084-0699(2007)12:5(513) PG 11 WC Engineering, Civil; Environmental Sciences; Water Resources SC Engineering; Environmental Sciences & Ecology; Water Resources GA 201JI UT WOS:000248826900009 ER PT J AU Ferrari, MR Miller, JR Russell, GL AF Ferrari, Michael R. Miller, James R. Russell, Gary L. TI Modeling changes in summer temperature of the Fraser River during the next century SO JOURNAL OF HYDROLOGY LA English DT Article DE climate change; Fraser River; hydrology; temperature; salmon ID CLIMATE-CHANGE; FLOW AB The Fraser River basin in British Columbia has significant environmental, economic and cultural importance. Healthy river conditions through sufficient flows and optimal temperatures are of paramount importance for the survival of Pacific salmon, which migrate upriver toward the headwaters to spawn near the end of their lives. Trends have been detected which indicate that the annual flow and summer temperature have been increasing since the middle of the last century. In this study we examine the observed trend in summer temperature of the Fraser River and compare it with temperatures calculated as part of a global climate model (GCM) simulation in which atmospheric greenhouse gases are increasing. We then use the GCM to consider how these trends might continue through the present century. Both the observations and model indicate that during the Last half of the 20th century, the summer temperature near the river mouth has been increasing at a rate of approximately 0.12 degrees C per decade in August. In this study we use an online method in which river temperatures are calculated directly as part of a GCM simulation and project how summer temperature near the mouth of the Fraser River might change by the end of the present century. The results indicate that between 2000 and 2100 river temperatures will increase in all summer months with a maximum increase of 0.14 degrees C per decade in August. This result is consistent with an offline modeling study by [Morrison, J., Quick, M.C., Goreman, M.G.G. 2002. Climate change in the Fraser River watershed: flow and temperature projections. Journal of Hydrology, 263, 230-244] in which they used output from two GCMS to drive a hydrologic model and predict future changes in river temperature and supports their contention that the timing and magnitude of the increase could be crucial for salmon migration. Future work can extend this analysis to other river systems in an effort to project the potential effects of climate change on the behavior of the world's large river basins, as well as identify the potential biological effects that may accompany these changes. (C) 2007 Elsevier B.V. All rights reserved. C1 Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA. Rutgers State Univ, Dept Marine & Coastal Sci, New Brunswick, NJ USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Ferrari, MR (reprint author), Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA. EM aeroculus@gmail.com NR 21 TC 38 Z9 40 U1 3 U2 21 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 J9 J HYDROL JI J. Hydrol. PD SEP 1 PY 2007 VL 342 IS 3-4 BP 336 EP 346 DI 10.1016/j.jhydrol.2007.06.002 PG 11 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 206IN UT WOS:000249177200012 ER PT J AU Shirron, PJ AF Shirron, Peter J. TI Cooling capabilities of adiabatic demagnetization refrigerators SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article AB The development of adiabatic demagnetization refrigerators (ADR) over the last decade has resulted in significant improvements in performance and ease of use, including continuous operation, relatively high cooling power (30-35 mu W at 100 mK), and cryogen-free operation. ADR systems are small, efficient, and require no auxiliary pumps or gas-handling systems. Consequently they are compact, convenient, low-cost options for ground-based research and instrument development. This paper presents an assessment of state-of-the-art ADRs in terms of temperature and cooling power capabilities, with emphasis on their applicability to quantum fluids and solids research. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Shirron, PJ (reprint author), NASA, Goddard Space Flight Ctr, Code 552, Greenbelt, MD 20771 USA. EM peter.shirron@nasa.gov NR 3 TC 9 Z9 9 U1 2 U2 8 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD SEP PY 2007 VL 148 IS 5-6 BP 915 EP 920 DI 10.1007/s10909-007-9441-7 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 190IJ UT WOS:000248052200073 ER PT J AU Devi, VM Benner, DC Brown, LR Miller, CE Toth, RA AF Devi, V. Malathy Benner, D. Chris Brown, L. R. Miller, C. E. Toth, R. A. TI Line mixing and speed dependence in CO2 at 6227.9 cm(-1) Constrained multispectrum analysis of intensities and line shapes in the 30013 <- 00001 band SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE cO(2); positions; intensities and pressure broadening; off-diagonal relaxation matrix element coefficients; line mixing; Lorentz widths; pressure shifts; near infrared; speed dependent line shape ID NEAR-INFRARED SPECTROSCOPY; 1.6 MU-M; CARBON-DIOXIDE; (CO2)-C-12-O-16; POSITIONS; STRENGTHS; AR; ATMOSPHERE; ACCURACY; WIDTHS AB Line position, intensity and line shape parameters (Lorentz widths, pressure shifts, line mixing, speed dependence) are reported for transitions of the 30013 <- 00001 band of (OCO)-O-16-C-12-O-16 (nu(0) = 6227.9 cm(-1)). The results are determined from 26 high-resolution, high signal-to-noise ratio spectra recorded at room temperature with the McMath-Pierce Fourier transform spectrometer. To minimize the systematic errors of the retrieved parameters, we constrained the multispectrum nonlinear least squares retrieval technique to use quantum mechanical expressions for the rovibrational energies and intensities rather than retrieving the individual positions and intensities line by line. Self- and air-broadened Lorentz width and pressure-induced shift, speed dependence and line mixing (off-diagonal relaxation matrix elements) coefficients were adjusted individually. Errors were further reduced by simultaneously fitting the interfering absorptions from the weak 30012 <- 00001 band of (OCO)-O-16-C-13-O-16 as well as the weak hot bands 31113 <- 01101, 32213 <- 02201, 40014 <- 10002 and 40013 <- 10001 of (OCO)-O-16-C-12-O-16 in this spectral window. This study complements our previous work on line mixing and speed dependence in the 30012 <- 00001 band (nu(0) = 6347.8 cm(-1)) [V.M. Devi, D.C. Benner, L.R. Brown, C.E. Miller, R.A. Toth, J. Mol. Spectrosc. 242 (2007) 90-117] and provides key data needed to improve atmospheric remote sensing Of CO2 (c) 2007 Elsevier Inc. All rights reserved. C1 Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Benner, DC (reprint author), Coll William & Mary, Dept Phys, Box 8795, Williamsburg, VA 23187 USA. EM dcbenn@wm.edu NR 30 TC 68 Z9 67 U1 0 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD SEP PY 2007 VL 245 IS 1 BP 52 EP 80 DI 10.1016/j.jms.2007.05.015 PG 29 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 214PH UT WOS:000249750100006 ER PT J AU Wey, CC Anderson, BE Wey, C Miake-Lye, RC Whitefield, P Howard, R AF Wey, Chowen C. Anderson, Bruce E. Wey, Changlie Miake-Lye, Richard C. Whitefield, Philip Howard, Robert TI Overview on the aircraft particle emissions experiment SO JOURNAL OF PROPULSION AND POWER LA English DT Article AB Conducted at the NASA Dryden Flight Research Center during April 2004, the Aircraft Particle Emissions Experiment systematically investigated the gas-phase and particle emissions from a CFM56-2C1 engine on NASA's DC-8 aircraft as functions of engine power, fuel composition, and exhaust-plume age. Emissions parameters were measured at 11 engine power settings ranging from idle to maximum thrust, in samples collected 1, 10, and 30 m downstream of the exhaust plane as the aircraft burned three fuels with different aromatic and sulfur contents. The land 10-m sampling rakes contained multiple gas and particle inlet probes to facilitate a study of the spatial variation of emissions across the engine exhaust plane. Gas-phase emission indices measured at 1 m were in good agreement with the engine certification data as well as with predictions provided by the engine company. However, at low power settings, trace-species emissions were observed to be highly dependent on ambient conditions and engine temperature. Nonvolatile particles emitted by the engine exhibited a log-normal size distribution that peaked between 15 and 40 nm, depending on engine power. Samples collected 30 m downstream of the engine exit plane exhibited a prominent nucleation mode, indicating that secondary aerosols composed of sulfuric acid and low-volatility organic species formed rapidly within the plume as it expanded and cooled. Black carbon emissions were a minimum at approach and a maximum at climb and takeoff engine power settings. Black carbon dominated total mass emissions at high thrust, whereas volatile particles contributed an equal or perhaps greater fraction at low- to midpower settings. Although variations in fuel aromatic content had no discernible impact on particle emissions, volatile particle number and mass concentrations in aged exhaust plumes were highly sensitive to the fuel sulfur content. C1 USA, Res Lab, Cleveland, OH 44135 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. QSS Grp Inc, Cleveland, OH 44135 USA. Aerodyne Res Inc, Billerica, MA 01821 USA. Univ Missouri, Rolla, MO 65409 USA. Arnold AF Base, Arnold Engn Dev Ctr, Tullahoma, TN 37389 USA. RP Wey, CC (reprint author), USA, Res Lab, Cleveland, OH 44135 USA. NR 18 TC 54 Z9 54 U1 1 U2 9 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2007 VL 23 IS 5 BP 898 EP 905 DI 10.2514/1.26406 PG 8 WC Engineering, Aerospace SC Engineering GA 213MH UT WOS:000249671200002 ER PT J AU Wey, T Liu, NS AF Wey, Thomas Liu, Nan-Suey TI Modeling jet engine aerosols in the postcombustor flow path and sampling system SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID NUCLEATION RATES; PARTICLES; PARAMETERIZATION; EMISSIONS; DYNAMICS; PARTEMIS; GROWTH; PLUMES AB Aircraft emissions contribute to climate change in the atmosphere and air pollution in the neighborhood of airports. Assessment of the magnitude of the environmental impact of these emissions calls for the combined use of measurements and modeling studies. This paper addresses the use of a computational-fluid-dynamics-based modeling and simulation tool that accounts for and integrates fluid dynamics, chemistry, and particle microphysics relevant to aircraft emissions. The models include sulfate and nitrate aerosol precursors, thermophoresis, coagulation, nucleation, soot activation, condensation/evaporation, and interaction between the gaseous species and the particles. The current capabilities are demonstrated by the results of several applications: the first stage of a high-pressure turbine, the sampling probes, the sampling lines, and a pressure-reduction chamber. They indicate that this modeling and simulation tool can be used to complement the experimental studies as well as to assist the development of sampling and measurement methodology for particle emissions. C1 NASA, John H Glenn Res Ctr Lewis Field, Combust Branch, Cleveland, OH 44135 USA. NR 33 TC 6 Z9 6 U1 2 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2007 VL 23 IS 5 BP 930 EP 941 DI 10.2514/1.24274 PG 12 WC Engineering, Aerospace SC Engineering GA 213MH UT WOS:000249671200006 ER PT J AU Knighton, WB Rogers, TM Anderson, BE Herndon, SC Yelvington, PE Miake-Lye, RC AF Knighton, Walter B. Rogers, Todd M. Anderson, Bruce E. Herndon, Scott C. Yelvington, Paul E. Miake-Lye, Richard C. TI Quantification of aircraft engine hydrocarbon emissions using proton transfer reaction mass Spectrometry SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID VOLATILE ORGANIC-COMPOUNDS; USE COMMERCIAL AIRCRAFT; IN-FLIGHT MEASUREMENT; ION FLOW TUBE; PTR-MS; PERFORMANCE; INDEXES; EXHAUST; O-2(+); RATIOS AB A proton transfer reaction mass spectrometer was used to measure the concentrations of selected volatile organic compounds in the exhaust of a commercial turbofan aircraft engine. Nine different compounds including methanol, acetaldehyde, acetic acid, benzene, toluene, phenol, styrene, naphthalene, and the methylnaphthalenes were identified as engine exhaust components that are free of spectral interferences and quantifiable by the proton transfer reaction mass spectrometer. The emission characteristics of the engine were examined as a function of engine power, fuel composition, and downstream distance from the engine. The hydrocarbon emission indices were found to be highly variable, upwards to a factor of 10 for the same nominal engine power setting. Although the magnitude of the HC emissions exhibited large variation, we observed that plots of the HC emission indices versus that of the emission index determined for formaldehyde (normalized plots) were linear and essentially independent of power setting and fuel composition, which suggests that the HC emissions scale together. The results of this study are critically examined and are shown to compare favorably with those of previous studies and serve to validate the proton transfer reaction mass spectrometer method as a reliable quantitative technique for online monitoring of selected hydrocarbon emissions within the engine exhaust matrix. C1 Montana State Univ, Dept Chem & Biochem, Bozeman, MT 59717 USA. NASA, Langley Res Ctr, Chem & Dynam Branch, Sci Directorate, Hampton, VA 23681 USA. Aerodyne Res Inc, Ctr Atomospher & Environm Chem, Billerica, MA 01821 USA. Aerodyne Res Inc, Ctr Aerothermodynam, Billerica, MA 01821 USA. RP Knighton, WB (reprint author), Montana State Univ, Dept Chem & Biochem, POB 173400, Bozeman, MT 59717 USA. NR 30 TC 32 Z9 33 U1 1 U2 11 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 EI 1533-3876 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2007 VL 23 IS 5 BP 949 EP 958 DI 10.2514/1.22965 PG 10 WC Engineering, Aerospace SC Engineering GA 213MH UT WOS:000249671200008 ER PT J AU DeBonis, JR AF DeBonis, James R. TI Progress toward large-eddy Simulations for prediction of realistic nozzle systems SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID NONREFLECTING BOUNDARY-CONDITIONS; FINITE-DIFFERENCE SCHEMES; REYNOLDS-NUMBER JET; RUNGE-KUTTA SCHEMES; COMPUTATIONAL ACOUSTICS; COMPLEX GEOMETRIES; AERODYNAMIC SOUND; LOW-DISSIPATION; NOISE; FLOWS C1 NASA, John H Glenn Res Ctr Lewis Field, Inlet & Nozzle Branch, Cleveland, OH 44135 USA. RP DeBonis, JR (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Inlet & Nozzle Branch, 21000 Brookpk Rd,Mail Stop 86-7, Cleveland, OH 44135 USA. NR 79 TC 11 Z9 11 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2007 VL 23 IS 5 BP 971 EP 980 DI 10.2514/1.24790 PG 10 WC Engineering, Aerospace SC Engineering GA 213MH UT WOS:000249671200010 ER PT J AU Goebel, DM Wirz, RE Katz, I AF Goebel, Dan M. Wirz, Richard E. Katz, Ira TI Analytical ion thruster discharge performance model SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID PLASMA PROPERTIES; CROSS-SECTIONS; GASES AB A particle and energy balance model of the plasma discharge in magnetic ring-cusp ion thrusters has been developed. The model follows prior work in the development of global zero-dimensional discharge models that use conservation of particles into and out of the thruster, conservation of energy into the discharge and out of the plasma in the form of charged particles to the walls and beam, and plasma radiation. The present model is significantly expanded over the prior art by closing the set of equations with self-consistent calculations of the internal neutral pressure, electron temperature, primary electron density, electrostatic ion confinement (due to the ring-cusp fields), plasma potential, discharge stability, and time-dependent behavior during recycling. The model only requires information on the thruster geometry, ion optics performance, and electrical inputs, such as discharge voltage and currents, to produce accurate performance curves of discharge loss vs mass utilization efficiency. The model has been benchmarked against several ion thrusters, and successfully predicts the thruster discharge loss as a function of mass utilization efficiency for a variety of thrusters. The discharge performance model will be described and results showing ion thruster performance and stability presented. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Goebel, DM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 32 TC 13 Z9 17 U1 1 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2007 VL 23 IS 5 BP 1055 EP 1067 DI 10.2514/1.26404 PG 13 WC Engineering, Aerospace SC Engineering GA 213MH UT WOS:000249671200020 ER PT J AU Mason, LS AF Mason, Lee S. TI Realistic specific power expectations for advanced radioisotope power systems SO JOURNAL OF PROPULSION AND POWER LA English DT Article AB Radioisotope power systems are being considered for a wide range of future NASA space science and exploration missions. Generally, radioisotope power systems offer the advantages of high reliability, long life, and predictable power production regardless of operating environment. Previous radioisotope power systems, in the form of radioisotope thermoelectric generators, have been used successfully on many NASA missions including Apollo, Viking, Voyager, and Galileo. NASA is currently evaluating design options for the next generation of radioisotope power systems. Of particular interest is the use of advanced, higher efficiency power conversion to replace the previous thermoelectric devices. Higher efficiency reduces the quantity of radioisotope fuel and potentially improves the radioisotope power systems specific power (watts per kilogram). Power conversion options include segmented thermoelectric, Stirling, Brayton, and thermophotovoltaic. This paper offers an analysis of the advanced 100 W-class radioisotope power system options and provides credible projections for specific power. Based on the analysis presented, radioisotope power system specific power values greater than 10 W/kg appear unlikely. C1 NASA, John H Glenn Res Ctr Lewis Field, Thermal Energy Convers Branch, Cleveland, OH 44135 USA. RP Mason, LS (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Thermal Energy Convers Branch, 21000 Brookpk Rd,MS301-2, Cleveland, OH 44135 USA. NR 4 TC 6 Z9 6 U1 1 U2 7 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD SEP-OCT PY 2007 VL 23 IS 5 BP 1075 EP 1079 DI 10.2514/1.26444 PG 5 WC Engineering, Aerospace SC Engineering GA 213MH UT WOS:000249671200022 ER PT J AU Iapaolo, M Godin-Beekmann, S Del Frate, F Casadio, S Petitdidier, M McDermid, IS Leblanc, T Swart, D Meijer, Y Hansen, G Stebel, K AF Iapaolo, M. Godin-Beekmann, S. Del Frate, F. Casadio, S. Petitdidier, M. McDermid, I. S. Leblanc, T. Swart, D. Meijer, Y. Hansen, G. Stebel, K. TI Gome ozone profiles retrieved by neural network techniques: A global validation with lidar measurements SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article ID MONITORING EXPERIMENT GOME; STRATOSPHERIC OZONE; ALGORITHM; SYSTEM AB Ozone profiles retrieved from Global Ozone Monitoring Experiment (GOME, flying on ERS-2 satellite) spectra from July 1995 to June 2003 by means of 2 independent neural network (NN) schemes have been validated with ozone lidar measurements performed at different stations belonging to the network for the detection of atmospheric composition changes (NDACC). The retrieval and the whole validation have been carried out by using the performances and resources of the European project Enabling Grid for E-sciencE (EGEE) and of a local Grid at the European Space Research Institute of the European Space Agency (ESRIN/ESA). Roughly 1800 collocated profiles have been found, in tropical, mid-latitude and high-latitude regions; for each lidar station the differences between GOME and lidar profiles have been evaluated and the global performance of the proposed NN approaches has been critically discussed. The results indicate the potentialities for obtaining reliable ozone field analysis on global scale, including detailed altitude resolved trend analysis. (C) 2007 Elsevier Ltd. All rights reserved. C1 UPMC, CNRS, Inst Pierre Simon Laplace, Serv Aeron, F-75252 Paris 05, France. Univ Roma Tor Vergata, Dipartimento Informat Sistemi & Produzione, I-00133 Rome, Italy. Karl Franzens Univ Graz, Inst Geophys, I-00044 Frascati, Italy. CNRS, Inst Pierre Simon Laplace, Ctr Etud Environm Terr & Planetaires, F-78140 Velizy Villacoublay, France. CALTECH, Table Mountain Facil, Jet Prop Lab, Wrightwood, CA 92397 USA. Natl Inst Publ Hlth & Environm, Lab Environm Monitoring, Environm & Safety Div, NL-3720 BA Bilthoven, Netherlands. Norwegian Inst Air Res, Polar Environm Ctr, NO-9296 Tromso, Norway. RP Godin-Beekmann, S (reprint author), UPMC, CNRS, Inst Pierre Simon Laplace, Serv Aeron, Boite 102,4 Pl Jussieu, F-75252 Paris 05, France. EM sophie.godin@aero.jussieu.fr RI Del Frate, Fabio/G-1413-2013; Stebel, Kerstin/F-6465-2013 OI Stebel, Kerstin/0000-0002-6935-7564 NR 21 TC 6 Z9 6 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD SEP PY 2007 VL 107 IS 1 BP 105 EP 119 DI 10.1016/j.jqsrt.2007.02.015 PG 15 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 182LK UT WOS:000247505900009 ER PT J AU Rinsland, CP Coheur, PF Herbin, H Clerbaux, C Boone, C Bernath, P Chiou, LS AF Rinsland, C. P. Coheur, P. F. Herbin, H. Clerbaux, C. Boone, C. Bernath, P. Chiou, L. S. TI Detection of elevated tropospheric hydrogen peroxide (H2O2) mixing ratios in atmospheric chemistry experiment (ACE) subtropical infrared solar occultation spectra SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE remote sensing; tropospheric chemistry; pollution; spectroscopy ID LINE-INTENSITIES; MODEL; C2H6; BAND; HOX; NOX; HCN; CO AB We report measurements of hydrogen peroxide (H2O2) profiles from infrared solar occultation spectra recorded at 0.02 cm(-1) resolution by the atmospheric chemistry experiment (ACE) during 2004 and 2005. Mixing ratios as high as 1.7 ppbv (1 ppbv = 1 x 10(-9) per unit volume) were measured in the subtropical troposphere. Back trajectories, fire count statistics, and simultaneous measurements of other species from the same occultation provide evidence that the elevated H2O2 mixing ratios originated from a young biomass-burning plume. The ACE time series show only a few cases with elevated H2O2 mixing ratios likely because of the short lifetime of H2O2 and the limited sampling during biomass-burning time periods. (c) 2007 Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. Univ Libre Bruxelles, Spectroscop Atmosph Chim Quant & Photophys, B-1050 Brussels, Belgium. Univ Paris 06, Inst Pierre Simon Laplace, Serv Aeron, Paris 06, France. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. Sci Syst & Applicat Inc, Hampton, VA 23666 USA. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Sci Directorate, Mail Stop 401A, Hampton, VA 23681 USA. EM c.p.rinsland@larc.nasa.gov; pfcoheur@ulb.ac.be; hherbin@ulb.ac.be; cathy.clerbaux@aero.jussieu.fr; cboone@acebox.uwaterloo.ca; bernath@uwaterloo.ca; l.s.chiou@larc.nasa.gov RI Bernath, Peter/B-6567-2012; clerbaux, cathy/I-5478-2013 OI Bernath, Peter/0000-0002-1255-396X; NR 27 TC 19 Z9 19 U1 0 U2 2 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 SEP PY 2007 VL 107 IS 2 BP 340 EP 348 DI 10.1016/j.jqsrt.2007.02.009 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 204PC UT WOS:000249055500011 ER PT J AU Johnston, CO Hollis, BR Sutton, K AF Johnston, Christopher O. Hollis, Brian R. Sutton, Kenneth TI Radiative heating methodology for the Huygens probe SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA/ASME 9th Joint Thermophysics and Heat Transfer Conference CY JUN 05-08, 2006 CL San Francisco, CA SP AIAA, ASME ID VISCOUS SHOCK-LAYER; CN; NONEQUILIBRIUM AB The radiative heating environment for the Huygens probe near peak heating conditions for Titan entry is investigated in this paper. The task of calculating the radiation-coupled flowfield, accounting for non-Boltzmann and non-optically thin radiation, is simplified to a rapid yet accurate calculation. This is achieved by using the viscous-shock-layer technique for the stagnation-line flowfield calculation and a modified smeared-rotational band model for the radiation calculation. These two methods provide a computationally efficient alternative to a Navier-Stokes flowfield and line-by-line radiation calculation. The results of the viscous-shock-layer technique are shown to provide an excellent comparison with the Navier-Stokes results of previous studies. It is shown that a conventional smeared-rotational hand approach is inadequate for the partially optically thick conditions present in the Huygens shock layer around the peak heating trajectory points. A simple modification is proposed to the smeared-rotational band model that improves its accuracy in these partially optically thick conditions. This modified approach, referred to as the smeared-rotational band corrected, is compared throughout this study with a detailed line-by-line calculation and is shown to compare within 5% in all cases. The smeared-rotational band corrected method requires many orders-of-magnitude less computational time than the line-by-line method, which makes it ideal for coupling to the flowfield. The application of a collisional-radiative model for determining the population of the CN electronic states, which govern the radiation for Huygens entry, is discussed and applied. The nonlocal absorption term in the collisional-radiative model is formulated in terms of an escape factor, which is then curve-fit with temperature. Although the curve fit is an approximation, it is shown to compare well with the exact escape factor calculation, which requires a computationally intensive iteration procedure. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Inst Natl Aerosp, Hampton, VA 24060 USA. RP Johnston, CO (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 34 TC 10 Z9 10 U1 1 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD SEP-OCT PY 2007 VL 44 IS 5 BP 993 EP 1002 DI 10.2514/1.26424 PG 10 WC Engineering, Aerospace SC Engineering GA 223YF UT WOS:000250411400001 ER PT J AU DeSmidt, HA Wang, KW Fang, H AF DeSmidt, H. A. Wang, K. W. Fang, H. TI Optimized Gore/Seam cable-actuated shape control of gossamer membrane reflectors SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 7th Gossamer Spacecraft Forum CY MAY 01-04, 2006 CL Newport, RI SP AIAA ID PRECISION AB This investigation explores the feasibility of using an active gore/seam cable-based control system to reduce global root mean square figure errors due to thermal loading and inflation effects (W error) in large, gossamer, inflatable membrane reflectors. Analysis is performed on an inflated spherical membrane with polyvinylidene-fluoride-actuated radial cables, for which the cable lengths and attachment points are designed via genetic algorithm optimization. It is found that through proper tailoring of the cable lengths, significant global root mean square figure-error reduction is achieved. Specifically, root mean square errors due to on-orbit thermal loading were reduced by approximately 75% with a 104-cable active gore/seam cable-control system that has a mass equal to 15% the original reflector. Sinailarly, W errors were reduced by approximately 95% with a 104-gore/seam cable-control system with a mass ratio of 12%. Finally, to deal with simultaneous W error and thermal loading with uncertain relative magnitudes, a hybrid gore/seam cable-control configuration based on a combination of independently optimized thermal and W-error cable patterns is considered. By adjusting the weights of a hybrid objective function, the gore/ seam cable-control system demonstrated robust shape-control performance for combined loading conditions. Because of the relatively lightweight designs and shape-control effectiveness, the gore/seam cable-shape-control concept seems promising for future gossamer reflector applications. C1 Univ Tennessee, Aerosp & Biomed Engn Dept, Knoxville, TN 37996 USA. Penn State Univ, Dept Mech & Nucl Engn, University Pk, PA 16802 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP DeSmidt, HA (reprint author), Univ Tennessee, Aerosp & Biomed Engn Dept, Knoxville, TN 37996 USA. NR 19 TC 5 Z9 5 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD SEP-OCT PY 2007 VL 44 IS 5 BP 1122 EP 1130 DI 10.2514/1.25109 PG 9 WC Engineering, Aerospace SC Engineering GA 223YF UT WOS:000250411400013 ER PT J AU Suzuki, M Ngo, Q Kitsuki, H Gleason, K Ominami, Y Yang, CY Yamada, T Cassell, AM Li, J AF Suzuki, Makoto Ngo, Quoc Kitsuki, Hirohiko Gleason, Kristofer Ominami, Yusuke Yang, Cary Y. Yamada, Toshishige Cassell, Alan M. Li, Jun TI Bright-field transmission imaging of carbon nanofibers on bulk substrate using conventional scanning electron microscopy SO JOURNAL OF VACUUM SCIENCE & TECHNOLOGY B LA English DT Article ID NANOTUBE; SINGLE; EMISSION; INTERCONNECT; CONTRAST; DEVICES; STAGE AB The authors present scanning transmission electron microscopy (STEM) of carbon nanofibers (CNFs) on a bulk substrate using conventional scanning electron microscopy (SEM) without specimen thinning. By utilizing the electron beam tilted >85 degrees from the substrate normal, bright-field STEM contrast is obtained for the CNFs on substrate with conventional SEM. Analysis of the observed contrast using Monte Carlo simulation shows that the weakly scattered electrons transmitted from the CNF are selectively enhanced by the largely tilted substrate and result in the observed STEM contrast. This mechanism provides a useful STEM imaging technique to investigate the internal structure of materials on bulk substrates without destructive specimen thinning. (C) 2007 American Vacuum Society. C1 Santa Clara Univ, Ctr Nanostruct, Santa Clara, CA 95053 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Suzuki, M (reprint author), Hitachi High Technol Corp, Ibaraki 3128504, Japan. EM suzuki-makoto@naka.hitachi-hitec.com RI Yamada, Toshishige/E-7834-2012; Li, Jun/H-7771-2013 OI Yamada, Toshishige/0000-0001-7145-9212; Li, Jun/0000-0002-3689-8946 NR 41 TC 3 Z9 3 U1 0 U2 3 PU A V S AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 1071-1023 J9 J VAC SCI TECHNOL B JI J. Vac. Sci. Technol. B PD SEP-OCT PY 2007 VL 25 IS 5 BP 1615 EP 1621 DI 10.1116/1.2775457 PG 7 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA 224FS UT WOS:000250433500013 ER PT J AU Abercromby, AFJ Amonette, WE Layne, CS Mcfarlin, BK Hinman, MR Paloski, WH AF Abercromby, Andrew F. J. Amonette, William E. Layne, Charles S. Mcfarlin, Brian K. Hinman, Martha R. Paloski, William H. TI Variation in neuromuscular responses during acute whole-body vibration exercise SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Article DE electromyography; posture; strength; damping; reflex ID SOFT-TISSUE RESONANCE; MUSCLE-SPINDLE; CONTRACTION; PERFORMANCE; STRENGTH; HUMANS; REFLEX; CAT AB Purpose: Leg muscle strength and power are increased after whole-body vibration (WBV) exercise. These effects may result from increased neuromuscular activation during WBV, however, previous studies of neuromuscular responses during WBV have not accounted for motion artifact. Methods: Sixteen healthy adults performed a series of static and dynamic unloaded squats with and without two different directions of WBV (rotational vibration, RV; and vertical vibration, VV, 30 Hz; 4 mm(p-p)). Activation of unilateral vastus lateralis, biceps femoris, gastrocnemius, and tibialis anterior was recorded using EMG. During RV and VV, increases in EMG relative to baseline were compared over a range of knee angles, contraction types (concentric, eccentric, isometric), and squatting types (static, dynamic). Results: After removing large, vibration-induced artifacts from EMG data using digital band-stop filters, neuromuscular activation of all four muscles increased significantly (P <= 0.05) during RV and VV. Average responses of the extensors were significantly greater during RV than VV, whereas responses of the tibialis anterior were significantly greater during VV than RV. For all four muscles, responses during static squatting were greater than or equal to responses during dynamic squatting, whereas responses during eccentric contractions were equal to or smaller than responses during concentric and isometric contractions. Neuromuscular responses of vastus lateralis, gastrocnemius, and tibialis anterior were affected by knee angle, with greatest responses at small knee angles. Conclusions: Motion artifacts should be removed from EMG data collected during WBV. We propose that neuromuscular responses during WBV may be modulated by leg muscle cocontraction as a postural control strategy and/or muscle tuning by the CNS intended to minimize soft-tissue vibration. C1 Univ Houston, Human Performance Lab, Houston, TX 77004 USA. Univ Houston, Lab Integrated Physiol, Houston, TX 77004 USA. Hardin Simmons Univ, Dept Phys Therapy, Abilene, TX 79601 USA. Natl Aeronaut & Space Adm, Human Adaptat & Countermeasures Div, Houston, TX USA. RP Abercromby, AFJ (reprint author), Wyle Labs Inc, 1290 Hercules Dr, Houston, TX 77058 USA. EM andrew.abercromby-l@nasa.gov NR 28 TC 140 Z9 143 U1 0 U2 11 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0195-9131 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD SEP PY 2007 VL 39 IS 9 BP 1642 EP 1650 DI 10.1249/mss.0b013618093f551 PG 9 WC Sport Sciences SC Sport Sciences GA 210GW UT WOS:000249445700027 PM 17805098 ER PT J AU Martins, Z Hofmann, BA Gnos, E Greenwood, RC Verchovsky, A Franchi, IA Jull, AJT Botta, O Glavin, DP Dworkin, JP Ehrenfreund, P AF Martins, Z. Hofmann, B. A. Gnos, E. Greenwood, R. C. Verchovsky, A. Franchi, I. A. Jull, A. J. T. Botta, O. Glavin, D. P. Dworkin, J. P. Ehrenfreund, P. TI Amino acid composition, petrology, geochemistry, C-14 terrestrial age and oxygen isotopes of the Shisr 033 CR chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CARBONACEOUS CHONDRITES; LIQUID-CHROMATOGRAPHY; PARENT BODY; METEORITES; HOT; CLASSIFICATION; ALLENDE; SAMPLES AB We have analyzed Shisr 033, a CR chondrite from the Omani desert, using several different analytical techniques designed to Study the degree of terrestrial alteration of this meteorite and also its petrologic classification. Bulk chemical analyses (including organic carbon and mean total H2O content) are consistent with a CR classification. Additionally, oxygen isotope analysis on a bulk sample indicates that Shisr 033 is of type CR2. Amino acid analysis using liquid chromatography with UV fluorescence detection (HPLC-FD) and liquid chromatography-time of flight-mass spectrometry (LC-ToF-MS) show that the absolute and the relative amino acid content of Shisr 033 is distinct from other carbonaceous chondrites. Oxygen isotope analysis of a phyllosilicate-rich dark inclusion shows that this inclusion is closer to CV3 or CO3 chondrites. The effects of terrestrial weathering in Shisr 033 are evident from the dark inclusion carbon isotopic data, bulk chemistry (through the elevated concentrations of Sr and Ba), and amino acid data, which suggests extensive amino acid contamination of the meteorite from the fall site soil. Nevertheless, Shisr 033 contains a small fraction of indigenous components, as indicated by the presence of the extraterrestrial amino acid alpha-aminoisobutyric acid (AIB) that was not detected in the Shisr soils. Finally, the terrestrial age of Shisr 033 was determined and is discussed in the context of high levels of contamination. C1 [Martins, Z.; Ehrenfreund, P.] Leiden Inst Chem, Astrobiol Lab, NL-2300 RA Leiden, Netherlands. [Hofmann, B. A.] Naturhistor Museum Burgergemeinde Bern, CH-3005 Bern, Switzerland. [Gnos, E.] Inst Geol Sci, CH-3012 Bern, Switzerland. [Greenwood, R. C.; Verchovsky, A.; Franchi, I. A.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. [Jull, A. J. T.] Univ Arizona, NSF Arizona Accelerator Mass Spectrometry Lab, Tucson, AZ 85721 USA. [Botta, O.; Glavin, D. P.; Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. RP Martins, Z (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, S Kensington Campus, London SW7 2AZ, England. EM z.martins@imperial.ac.uk RI Glavin, Daniel/D-6194-2012; Martins, Zita/H-4860-2015; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Martins, Zita/0000-0002-5420-1081; Dworkin, Jason/0000-0002-3961-8997 NR 45 TC 27 Z9 27 U1 0 U2 5 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2007 VL 42 IS 9 BP 1581 EP 1595 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 244MB UT WOS:000251868900008 ER PT J AU Connolly, HC Smith, C Benedix, G Folco, L Righter, K Zipfel, J Yamaguchi, A Aoudjehane, HC AF Connolly, Harold C., Jr. Smith, Caroline Benedix, Gretchen Folco, Luigi Righter, Kevin Zipfel, Jutta Yamaguchi, Akira Chennaoui Aoudjehane, Hasnaa TI The Meteoritical Bulletin, no. 92, 2007 September SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CLASSIFICATION AB In this edition of The Meteoritical Bulletin, 1394 recognized meteorites are reported, 27 from specific locations within Africa, 133 from Northwest Africa, 1227 from Antarctica (from ANSMET, PNRA, and PRIC expeditions), and 7 from Asia. The Meteoritical Bulletin announces the approval of four new names series by the Nomenclature Committee of the Meteoritical Society, two from Africa and one from Asia, including At Haggounia, from At Haggounia, Morocco, which is projected to be on the order of 3 metric tons of material related to enstatite chondrites and aubrites. Approved are two falls from Africa, Bassikounou (Mauritania) and Gashua (Nigeria). Approved from areas other than Antarctica are one lunar, two Martian, 32 other achondrites, three mesosiderites, two pallasites, one CM, two CK, one CR2, two CV3, one CR2, and four R chondrites. The Nomenclature Committee of the Meteoritical Society announces 48 newly approved relict meteorites from two new name series, Osterplana and Gullhogen (both from Sweden). C1 [Connolly, Harold C., Jr.] CUNY, Kingsborough Community Coll, Grad Sch, Dept Phys Sci, Brooklyn, NY 11210 USA. [Connolly, Harold C., Jr.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Connolly, Harold C., Jr.] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA. [Smith, Caroline; Benedix, Gretchen] Nat Hist Museum, Dept Mineral, London SW7 5BD, England. [Folco, Luigi] Museo Nazl Antartide, I-53100 Siena, Italy. [Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Code ST, Houston, TX 77058 USA. [Zipfel, Jutta] Forschungsinst Naturmuseum Senckenberg, Sekt Meteoritenforsch, D-60325 Frankfurt, Germany. [Yamaguchi, Akira] Natl Inst Polar Res, Antarctic Meteorite Res Ctr, Tokyo 1738515, Japan. [Chennaoui Aoudjehane, Hasnaa] Univ Hassan II Casablanca, Fac Sci, Dept Geol, Maarif, Casablanca, Morocco. RP Connolly, HC (reprint author), CUNY, Kingsborough Community Coll, Grad Sch, Dept Phys Sci, 2001 Oriental Blvd, Brooklyn, NY 11210 USA. EM meteorite@kingsborough.edu OI Benedix, Gretchen/0000-0003-0990-8878 NR 6 TC 22 Z9 23 U1 1 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2007 VL 42 IS 9 BP 1647 EP 1694 PG 48 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 244MB UT WOS:000251868900012 ER PT J AU Oates, SR De Pasquale, M Page, MJ Blustin, AJ Zane, S McGowan, K Mason, KO Poole, TS Schady, P Roming, PWA Page, KL Falcone, A Gehrels, N AF Oates, S. R. De Pasquale, M. Page, M. J. Blustin, A. J. Zane, S. McGowan, K. Mason, K. O. Poole, T. S. Schady, P. Roming, P. W. A. Page, K. L. Falcone, A. Gehrels, N. TI The two-component afterglow of Swift GRB 050802 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-rays : bursts ID GAMMA-RAY BURSTS; ENERGY INJECTION; LIGHT CURVES; THEORETICAL IMPLICATIONS; DISSIPATION; TELESCOPE; EVOLUTION; EMISSION; OUTFLOWS; MODELS AB This paper investigates GRB 050802, one of the best examples of a Swift gamma-ray burst afterglow that shows a break in the X-ray light curve, while the optical counterpart decays as a single power law. This burst has an optically bright afterglow of 16.5 mag, detected throughout the 170-650 nm spectral range of the Ultraviolet and Optical Telescope (UVOT) onboard Swift. Observations began with the X-ray Telescope and UVOT telescopes 286 s after the initial trigger and continued for 1.2 x 10(6) s. The X-ray light curve consists of three power-law segments: a rise until 420 s, followed by a slow decay with alpha= 0.63 +/- 0.03 until 5000 s, after which, the light curve decays faster with a slope of alpha(3)= 1.59 +/- 0.03. The optical light curve decays as a single power law with alpha(O) = 0.82 +/- 0.03 throughout the observation. The X-ray data on their own are consistent with the break at 5000 s being due to the end of energy injection. Modelling the optical to X-ray spectral energy distribution, we find that the optical afterglow cannot be produced by the same component as the X-ray emission at late times, ruling out a single-component afterglow. We therefore considered two-component jet models and find that the X-ray and optical emission is best reproduced by a model in which both components are energy injected for the duration of the observed afterglow and the X-ray break at 5000 s is due to a jet break in the narrow component. This bright, well-observed burst is likely a guide for interpreting the surprising finding of Swift that bursts seldom display achromatic jet breaks. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Oates, SR (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM sro@mssl.ucl.ac.uk RI Gehrels, Neil/D-2971-2012 NR 43 TC 27 Z9 27 U1 1 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2007 VL 380 IS 1 BP 270 EP 280 DI 10.1111/j.1365-2966.2007.12054.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 209YC UT WOS:000249422900040 ER PT J AU Cucurull, L Derber, JC Treadon, R Purser, RJ AF Cucurull, L. Derber, J. C. Treadon, R. Purser, R. J. TI Assimilation of global positioning system radio occultation observations into NCEP's global data assimilation system SO MONTHLY WEATHER REVIEW LA English DT Article ID NUMERICAL WEATHER PREDICTION; LOW-EARTH-ORBIT; ATMOSPHERE; IMPACT; INVERSION; SIGNALS AB The Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) mission launched six small satellites in April 2006, each carrying a GPS radio occultation (RO) receiver. At final orbit, COSMIC will provide similar to 2500-3000 RO soundings per day uniformly distributed around the globe in near-real time. In preparation for the assimilation of COSMIC data in an operational framework, the NCEP/Environmental Modeling Center (EMC) has successfully developed the capability of assimilating profiles of refractivity and bending angle. Each forward operator has been implemented with its own quality control and error characterization. In this paper, the infrastructure developed at NCEP/EMC to assimilate GPS RO observations, including forward models, observational and representativeness errors, and quality control procedures, is described. The advantages of using a forward operator for bending angle versus refractivity are discussed and some preliminary results on the benefits of the GPS RO in weather analysis and forecasts are presented. The different strategies adopted at NCEP/EMC to assimilate GPS RO data are aimed to select the most appropriate forward operator in the operational data assimilation system when COSMIC products are stable and routinely available to the Numerical Weather Centers. In the meantime, data from the Challenging Minisatellite Payload (CHAMP) satellite is available in non-real time and has been used in the assimilation tests to examine the potential benefits of the GPS RO-derived products. In the preliminary results presented in this study, the use of GPS RO observations slightly improves anomaly correlation scores for temperature (by similar to 0.01-0.03) in the Southern Hemisphere and Tropics throughout the depth of the atmosphere while a slight degradation is found in the upper troposphere and stratosphere in the Northern Hemisphere. However, significant reduction of the temperature and humidity biases is found for all latitudes. The benefits from assimilating GPS RO data also extend to other fields, such as 500-hPa geopotential heights and tropical winds, demonstrating the potential use of GPS RO data in operational forecasting. C1 NASA, NOAA, DOD Joint Ctr Satellite Data Assimilat, Washington, DC 20546 USA. Univ Corp Atmospher Res, Boulder, CO USA. Natl Ctr Environm Predict Environm Modeling Ctr, Washington, DC USA. Sci Applicat Int Corp, Beltsville, MD USA. RP Cucurull, L (reprint author), NOAA, NWS, NCEP, EMC, W-NP2,5200 Auth Rd,Room 207, Suitland, MD 20746 USA. EM lidia.cucurull@noaa.gov RI Cucurull, Lidia/E-8900-2015 NR 26 TC 56 Z9 57 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD SEP PY 2007 VL 135 IS 9 BP 3174 EP 3193 DI 10.1175/MWR3461.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 208WO UT WOS:000249350100010 ER PT J AU Dwek, E Galliano, F Jones, AP AF Dwek, E. Galliano, F. Jones, A. P. TI The origin and evolution of dust in high-redshift galaxies SO NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-GENERAL PHYSICS RELATIVITY ASTRONOMY AND MATHEMATICAL PHYSICS AND METHODS LA English DT Article ID QUASARS; EMISSION; GAS AB Dusty hyperluminous galaxies in the early Universe provide unique environments for studying the role of massive stars in the formation and destruction of (lust;. At redshifts above. 6; when the Universe was less than 1 Gy old, dust could have only condensed in the explosive ejecta, of Type II supernovae (SNe), since most of the progenitors of the AGB stars; the major alternative source of interstellar (lust; did not have time to evolve off the main sequence. We present analytical models for the evolution of the gas, (lust, and metals in high-redshift galaxies, with a special application to SDSS J1148+5251, a hyperhuminous quasar at z = 6.4 hereafter referred to as J1148+5251. We show that an average SN must condense at least 1 M-circle dot of dust to account for the mass of dust in this object, when grain destruction by supernova remnants (SNRs) is taken into account. This required Yield is in excess of similar to 0.05M(circle dot), the largest; mass of dust; inferred from infrared observations of Case A. If the yield of Case A is typical, then other processes; such as accretion onto pre-existing grains in molecular clouds are needed to produce the mass of dust in J1148+5251. For such process to be effective; SNR must significantly increase; presumably by non-evaporative grain-grain collisions during the late stages of their evolution, the number of nucleation centers onto which refractory elements can condense in molecular clouds. C1 [Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Galliano, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Jones, A. P.] Inst Astrophys Spatiale, F-91405 Orsay, France. RP Dwek, E (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. FU NASA's [LTSA 03-0000-065]; National Research Council (NRC); Oak Ridge Associated Universities (ORAU) at NASA Goddard Space Flight Center FX This work was supported by NASA's LTSA 03-0000-065. The work of FG was supported by Research Associateship awards from the National Research Council (NRC) and from the, Oak Ridge Associated Universities (ORAU) at NASA Goddard Space Flight Center. NR 16 TC 12 Z9 12 U1 0 U2 0 PU SOC ITALIANA FISICA PI BOLOGNA PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY SN 1594-9982 J9 NUOVO CIMENTO B JI Nouvo Cimento Soc. Ital. Fis. B-Gen. Phys. Relativ. Astron. Math. Phys. Methods PD SEP-NOV PY 2007 VL 122 IS 9-11 BP 959 EP 966 DI 10.1393/ncb/i2008-10427-8 PG 8 WC Physics, Multidisciplinary SC Physics GA 345GZ UT WOS:000258985600005 ER PT J AU Benford, DJ Lauer, TR AF Benford, D. J. Lauer, T. R. TI Measuring cosmic expansion and large-scale structure with Destiny SO NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-GENERAL PHYSICS RELATIVITY ASTRONOMY AND MATHEMATICAL PHYSICS AND METHODS LA English DT Article AB Destiny is a simple direct, low-cost, mission to determine, the properties of dark energy by obtaining a, cosmologically Deep Supernova (SN) type la Hubble diagram and by measuring the large-scale mass power spectrum over time. Its science instrument is a. 1.65 m space telescope, featuring a hear-infrared survey camera/spectrometer with a large field of view. During its first two years, Destiny will detect, observe; acid characterize > 3000 SN la events over the redshift interval 0.4 < z < 1.7, thereby constructing a high-precision Hubble diagram to constrain the dark-energy equation of state. Destiny will be used in its third year as a, high-resolution, wide-field imager to conduct a weak lensing survey covering > 600 square degrees to measure the large-scale mass power spectrum. The combination of surveys is much more powerful than either technique on its own, and will have an order of magnitude greater sensitivity than near-future projects. C1 [Benford, D. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Lauer, T. R.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Benford, DJ (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 NR 2 TC 0 Z9 0 U1 0 U2 0 PU SOC ITALIANA FISICA PI BOLOGNA PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY SN 1594-9982 J9 NUOVO CIMENTO B JI Nouvo Cimento Soc. Ital. Fis. B-Gen. Phys. Relativ. Astron. Math. Phys. Methods PD SEP-NOV PY 2007 VL 122 IS 9-11 BP 1227 EP 1230 DI 10.1393/ncb/i2008-10515-9 PG 4 WC Physics, Multidisciplinary SC Physics GA 345GZ UT WOS:000258985600043 ER PT J AU Sonneborn, G Shull, JM Danforth, CW Moos, HW AF Sonneborn, G. Shull, J. M. Danforth, C. W. Moos, H. W. TI Baryonic content of the warm-hot intergalactic medium at low redshift SO NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-GENERAL PHYSICS RELATIVITY ASTRONOMY AND MATHEMATICAL PHYSICS AND METHODS LA English DT Article ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; ABSORBERS; HI AB This paper summarizes the largest survey to date (Danforth and Shull 2008) of the intergalactic medium (IGM) at low redshift, utilizing data from the Far Ultraviolet Spectroscopic Explorer and Hubble Space Telescope satellites. The IGM was detected in absorption against background AGN at z < 0.4. The survery identifies 650 Ly alpha and 83 O VI absorbers. O VI has a steeper power slope than H I (dN/dz proportional to N-beta, beta(O) (VI) similar to 2, beta(H) (1) = 1.7). Approximately 40% of baryons at low redshift are accounted for in the IGM (30% in the Ly alpha forest, 10% in the warm-hot IGM). O VI 1032-38 angstrom and N V 1238-42 angstrom absorbers are reliable WHIM tracers and are inconsistent with photoionization. The O VI transition is currently a much better WHIM tracer (N similar to 100) than X-ray O VIII detections (N similar to 1-2). The O VI detection frequency (dN/dz) implies metal transport out to 250-300 kpc from dwarf galaxies (L = 0.03 L*). C1 [Sonneborn, G.] NASA, Goddard Space Flight Ctr, Lab Observ Cosmol, Greenbelt, MD 20771 USA. [Shull, J. M.; Danforth, C. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Moos, H. W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Sonneborn, G (reprint author), NASA, Goddard Space Flight Ctr, Lab Observ Cosmol, Code 665, Greenbelt, MD 20771 USA. RI Sonneborn, George/D-5255-2012 NR 8 TC 0 Z9 0 U1 0 U2 0 PU SOC ITALIANA FISICA PI BOLOGNA PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY SN 1594-9982 J9 NUOVO CIMENTO B JI Nouvo Cimento Soc. Ital. Fis. B-Gen. Phys. Relativ. Astron. Math. Phys. Methods PD SEP-NOV PY 2007 VL 122 IS 9-11 BP 1307 EP 1310 DI 10.1393/ncb/i2008-10478-9 PG 4 WC Physics, Multidisciplinary SC Physics GA 345GZ UT WOS:000258985600060 ER PT J AU Staguhn, JG Dwek, E Benford, DJ Moseley, SH Sharp, EH AF Staguhn, J. G. Dwek, E. Benford, D. J. Moseley, S. H. Sharp, E. H. TI Science case for a 2 mm bolometer camera optimized for surveys of dusty galaxies in the high-redshift Universe SO NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-GENERAL PHYSICS RELATIVITY ASTRONOMY AND MATHEMATICAL PHYSICS AND METHODS LA English DT Article ID INFRARED ASTRONOMY; ARRAYS; FIELD AB We present results from our galaxy count models that demonstrate the scientific capabilities of high-sensitivity 2 mm wavelengths observations. These results motivated us to build the bolometer camera GISMO (the Goddard-Iran Superconducting Millimeter Observer) for operation in the 2 mm atmospheric window at the IRAM 30 m telescope, where it was successfully fielded on November, 2007. The instrument uses and 8 x 16 pixel planar array of multiplexed TES bolometers that provide a noise equivalent power of 3 x 10(-17)W/root Hz. The major scientific driver for this instrument is to provide the IRAM 30 m telescope with the capability to rapidly observe galactic and extragalactic dust emission, in particular from high-z ULIRGs and quasars even in relatively poor weather. Our models predict that in a dark-sky survey with GISMO virtually all galaxies that will be detected are at a redshift of z > 2. C1 [Staguhn, J. G.; Dwek, E.; Benford, D. J.; Moseley, S. H.; Sharp, E. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Staguhn, J. G.] Univ Maryland, College Pk, MD 20742 USA. [Sharp, E. H.] GST, Greenbelt, MD USA. RP Staguhn, JG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Benford, Dominic/D-4760-2012; Moseley, Harvey/D-5069-2012; Dwek, Eli/C-3995-2012 OI Benford, Dominic/0000-0002-9884-4206; FU NSF [AST 0705185] FX This work was supported in part by NSF Grant AST 0705185. NR 7 TC 3 Z9 3 U1 0 U2 0 PU SOC ITALIANA FISICA PI BOLOGNA PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY SN 1594-9982 J9 NUOVO CIMENTO B JI Nouvo Cimento Soc. Ital. Fis. B-Gen. Phys. Relativ. Astron. Math. Phys. Methods PD SEP-NOV PY 2007 VL 122 IS 9-11 BP 1311 EP 1314 DI 10.1393/ncb/i2008-10479-8 PG 4 WC Physics, Multidisciplinary SC Physics GA 345GZ UT WOS:000258985600061 ER PT J AU Mohageg, M Savchenkov, A Maleki, L AF Mohageg, Makan Savchenkov, Anatohy Maleki, Lute TI Coherent backscattering in lithium niobate whispering-gallery-mode resonators SO OPTICS LETTERS LA English DT Article ID MICROSPHERES; SCATTERING; FILTER AB Splitting of high-Q whispering gallery modes into a doublet of counterpropagating modes was observed in a resonator fabricated from LiNbO3. An energy-transfer rate of 10 MHz was calculated by measuring the frequency detuning of the doublet structure. The splitting rate is also used to calculate the maximum variation in the internal index of refraction over one wavelength, which is of the order of 10(-7). This shows that the mechanical process used to fabricate whispering-gallery-mode resonators from LiNbO3 is sufficient to achieve material-limited quality factors. (c) 2007 Optical Society of America. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mohageg, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM makan.mohageg@gmail.com NR 16 TC 4 Z9 4 U1 2 U2 10 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD SEP 1 PY 2007 VL 32 IS 17 BP 2574 EP 2576 DI 10.1364/OL.32.002574 PG 3 WC Optics SC Optics GA 216VV UT WOS:000249908000037 PM 17767309 ER PT J AU Nichol, J King, B Quattrochi, D Dowman, I Ehlers, M Ding, XL AF Nichol, Janet King, Bruce Quattrochi, Dale Dowman, Ian Ehlers, Manfred Ding, Xiaoli TI Earth Observation for Urban Planning and Management - State of the art and recommendations for application of Earth Observation in Urban Planning SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Editorial Material ID HEAT ISLANDS; HONG-KONG C1 Hong Kong Polytech Univ, Dept Land Surveying & Geoinformat, Kowloon, Hong Kong, Peoples R China. NASA, Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA. Univ London, Univ Coll, Dept Geomat Engn, London WC1E 7HU, England. Univ Osnabrueck, IGF, Inst Geoinformat & Remote Sensing, Osnabruck, Germany. RP Nichol, J (reprint author), Hong Kong Polytech Univ, Dept Land Surveying & Geoinformat, Kowloon, Hong Kong, Peoples R China. RI NICHOL, Janet /C-6780-2009; Ding, Xiaoli/K-4596-2013; Nichol, Janet/A-1442-2014; King, Bruce/C-1120-2008 OI Ding, Xiaoli/0000-0002-5733-3629; Nichol, Janet/0000-0003-4015-893X; King, Bruce/0000-0002-2651-5358 NR 29 TC 15 Z9 15 U1 1 U2 5 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD SEP PY 2007 VL 73 IS 9 BP 973 EP 979 PG 7 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 207EP UT WOS:000249234700001 ER PT J AU DiRienzi, J Drachman, RJ AF DiRienzi, Joseph Drachman, Richard J. TI Possible high-lying resonances in the positronium-hydrogen system SO PHYSICAL REVIEW A LA English DT Article ID SCATTERING; HYDRIDE; STATES AB We were previously successful in representing a series of low-lying Ps + H scattering resonances as due to quasibound Coulomb states in the closed-channel e(+) + H- system. Here we investigate the analogous Coulomb states of Ps(-) + H+, which are also accessible from the Ps + H scattering system, but at considerably higher collision energies. We locate several such states and suggest that they may be scattering resonances, but because there are many open-channel thresholds lying below they may have large widths and shifts. C1 Coll Notre Dame Maryland, Baltimore, MD 21210 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP DiRienzi, J (reprint author), Coll Notre Dame Maryland, Baltimore, MD 21210 USA. NR 15 TC 5 Z9 5 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD SEP PY 2007 VL 76 IS 3 AR 032705 DI 10.1103/PhysRevA.76.032705 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 215CN UT WOS:000249786000087 ER PT J AU Abbott, B Abbott, R Adhikari, R Agresti, J Ajith, P Allen, B Amin, R Anderson, B Anderson, WG Arain, M Araya, M Armandula, H Ashley, M Aston, S Aufmuth, P Aulbert, C Babak, S Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barton, MA Bayer, K Belczynski, K Betzwieser, J Beyersdorf, PT Bhawal, B Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, K Blackburn, L Blair, D Bland, B Bogenstahl, J Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, A Brown, DA Bullington, A Bunkowski, A Buonanno, A Burmeister, O Busby, D Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cao, J Cardenas, L Casey, MM Castaldi, G Cepeda, C Chalkey, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Chiadini, F Chin, D Chin, E Chow, J Christensen, N Clark, J Cochrane, P Cokelaer, T Colacino, CN Coldwell, R Conte, R Cook, D Corbitt, T Coward, D Coyne, D Creighton, JDE Creighton, TD Croce, RP Crooks, DRM Cruise, AM Cumming, A Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Debra, D Degallaix, J Degree, M Demma, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Az, MD' Dickson, J Di Credico, A Diederichs, G Dietz, A Doomes, EE Drever, RWP Dumas, JC Dupuis, RJ Dwyer, JG Ehrens, P Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Fan, Y Fazi, D Fejer, MM Finn, LS Fiumara, V Fotopoulos, N Franzen, A Franzen, KY Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Garofoli, J Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, L Gonzalez, G Gossler, S Grant, A Gras, S Gray, C Gray, M Greenhalgh, J Gretarsson, AM Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, R Hage, B Hammer, D Hanna, C Hanson, J Harms, J Harry, G Harstad, E Hayler, T Heefner, J Heng, IS Heptonstall, A Heurs, M Hewitson, M Hild, S Hirose, E Hoak, D Hosken, D Hough, J Howell, E Hoyland, D Huttner, SH Ingram, D Innerhofer, E Ito, M Itoh, Y Ivanov, A Jackrel, D Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kamat, S Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalili, FY Kim, C King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, RK Kozak, D Krishnan, B Kwee, P Lam, PK Landry, M Lantz, B Lazzarini, A Lee, B Lei, M Leiner, J Leonhardt, V Leonor, I Libbrecht, K Lindquist, P Lockerbie, NA Longo, M Lormand, M Lubinski, M Lueck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Malec, M Mandic, V Marano, S Marka, S Markowitz, J Maros, E Martin, I Marx, JN Mason, K Matone, L Matta, V Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McKenzie, K McNabb, JWC McWilliams, S Meier, T Melissinos, A Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, CJ Meyers, D Mikhailov, E Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Mohanty, S Moreno, G Mossavi, K MowLowry, C Moylan, A Mudge, D Mueller, G Mukherjee, S Muller-Ebhardt, H Munch, J Murray, P Myers, E Myers, J Nash, T Newton, G Nishizawa, A Numata, K O'Reilly, B O'Shaughnessy, R Ottaway, DJ Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Patel, P Pedraza, M Penn, S Pierro, V Pinto, IM Pitkin, M Pletsch, H Plissi, MV Postiglione, F Prix, R Quetschke, V Raab, F Rabeling, D Radkins, H Rahkola, R Rainer, N Rakhmanov, M Rawlins, K Ray-Majumder, S Re, V Rehbein, H Reid, S Reitze, DH Ribichini, L Riesen, R Riles, K Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rodriguez, A Rogan, AM Rollins, J Romano, JD Romie, J Route, R Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Sakata, S Samidi, M de la Jordana, LS Sandberg, V Sannibale, V Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P Schediwy, S Schilling, R Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Shawhan, P Shoemaker, DH Sibley, A Sidles, JA Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Somiya, K Strain, KA Strom, DM Stuver, A Summerscales, TZ Sun, KX Sung, M Sutton, PJ Takahashi, H Tanner, DB Tarallo, M Taylor, R Taylor, R Thacker, J Thorne, KA Thorne, KS Thuring, A Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Tyler, W Ugolini, D Ungarelli, C Urbanek, K Vahlbruch, H Vallisneri, M Van Den Broeck, C Varvella, M Vass, S Vecchio, A Veitch, J Veitch, P Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, R Watts, K Webber, D Weidner, A Weinert, M Weinstein, A Weiss, R Wen, S Wette, K Whelan, JT Whitbeck, DM Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Yunes, N Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, M zur Muhlen, H Zweizig, J AF Abbott, B. Abbott, R. Adhikari, R. Agresti, J. Ajith, P. Allen, B. Amin, R. Anderson, B. Anderson, W. G. Arain, M. Araya, M. Armandula, H. Ashley, M. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Ballmer, S. Bantilan, H. Barish, B. C. Barker, C. Barker, D. Barr, B. Barriga, P. Barton, M. A. Bayer, K. Belczynski, K. Betzwieser, J. Beyersdorf, P. T. Bhawal, B. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, K. Blackburn, L. Blair, D. Bland, B. Bogenstahl, J. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brooks, A. Brown, D. A. Bullington, A. Bunkowski, A. Buonanno, A. Burmeister, O. Busby, D. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. Cantley, C. A. Cao, J. Cardenas, L. Casey, M. M. Castaldi, G. Cepeda, C. Chalkey, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Chiadini, F. Chin, D. Chin, E. Chow, J. Christensen, N. Clark, J. Cochrane, P. Cokelaer, T. Colacino, C. N. Coldwell, R. Conte, R. Cook, D. Corbitt, T. Coward, D. Coyne, D. Creighton, J. D. E. Creighton, T. D. Croce, R. P. Crooks, D. R. M. Cruise, A. M. Cumming, A. Dalrymple, J. D'Ambrosio, E. Danzmann, K. Davies, G. Debra, D. Degallaix, J. Degree, M. Demma, T. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Az, M. Di ' Dickson, J. Di Credico, A. Diederichs, G. Dietz, A. Doomes, E. E. Drever, R. W. P. Dumas, J.-C. Dupuis, R. J. Dwyer, J. G. Ehrens, P. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Fan, Y. Fazi, D. Fejer, M. M. Finn, L. S. Fiumara, V. Fotopoulos, N. Franzen, A. Franzen, K. Y. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Garofoli, J. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. Gonzalez, G. Gossler, S. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, J. Gretarsson, A. M. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, R. Hage, B. Hammer, D. Hanna, C. Hanson, J. Harms, J. Harry, G. Harstad, E. Hayler, T. Heefner, J. Heng, I. S. Heptonstall, A. Heurs, M. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hosken, D. Hough, J. Howell, E. Hoyland, D. Huttner, S. H. Ingram, D. Innerhofer, E. Ito, M. Itoh, Y. Ivanov, A. Jackrel, D. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kamat, S. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalili, F. Ya. Kim, C. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. K. Kozak, D. Krishnan, B. Kwee, P. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lee, B. Lei, M. Leiner, J. Leonhardt, V. Leonor, I. Libbrecht, K. Lindquist, P. Lockerbie, N. A. Longo, M. Lormand, M. Lubinski, M. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Malec, M. Mandic, V. Marano, S. Marka, S. Markowitz, J. Maros, E. Martin, I. Marx, J. N. Mason, K. Matone, L. Matta, V. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McKenzie, K. McNabb, J. W. C. McWilliams, S. Meier, T. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messaritaki, E. Messenger, C. J. Meyers, D. Mikhailov, E. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Mohanty, S. Moreno, G. Mossavi, K. MowLowry, C. Moylan, A. Mudge, D. Mueller, G. Mukherjee, S. Mueller-Ebhardt, H. Munch, J. Murray, P. Myers, E. Myers, J. Nash, T. Newton, G. Nishizawa, A. Numata, K. O'Reilly, B. O'Shaughnessy, R. Ottaway, D. J. Overmier, H. Owen, B. J. Pan, Y. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. Plissi, M. V. Postiglione, F. Prix, R. Quetschke, V. Raab, F. Rabeling, D. Radkins, H. Rahkola, R. Rainer, N. Rakhmanov, M. Rawlins, K. Ray-Majumder, S. Re, V. Rehbein, H. Reid, S. Reitze, D. H. Ribichini, L. Riesen, R. Riles, K. Rivera, B. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rodriguez, A. Rogan, A. M. Rollins, J. Romano, J. D. Romie, J. Route, R. Rowan, S. Ruediger, A. Ruet, L. Russell, P. Ryan, K. Sakata, S. Samidi, M. de la Jordana, L. Sancho Sandberg, V. Sannibale, V. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Saulson, P. R. Savage, R. Savov, P. Schediwy, S. Schilling, R. Schnabel, R. Schofield, R. Schutz, B. F. Schwinberg, P. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Shawhan, P. Shoemaker, D. H. Sibley, A. Sidles, J. A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Somiya, K. Strain, K. A. Strom, D. M. Stuver, A. Summerscales, T. Z. Sun, K.-X. Sung, M. Sutton, P. J. Takahashi, H. Tanner, D. B. Tarallo, M. Taylor, R. Taylor, R. Thacker, J. Thorne, K. A. Thorne, K. S. Thuering, A. Tinto, M. Tokmakov, K. V. Torres, C. Torrie, C. Traylor, G. Trias, M. Tyler, W. Ugolini, D. Ungarelli, C. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van Den Broeck, C. Varvella, M. Vass, S. Vecchio, A. Veitch, J. Veitch, P. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, H. Ward, R. Watts, K. Webber, D. Weidner, A. Weinert, M. Weinstein, A. Weiss, R. Wen, S. Wette, K. Whelan, J. T. Whitbeck, D. M. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, L. Willke, B. Wilmut, I. Winkler, W. Wipf, C. C. Wise, S. Wiseman, A. G. Woan, G. Woods, D. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Yunes, N. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. zur Muehlen, H. Zweizig, J. CA LIGO Sci Collaboration TI Search for gravitational wave radiation associated with the pulsating tail of the SGR 1806 20 hyperflare of 27 December 2004 using LIGO SO PHYSICAL REVIEW D LA English DT Article ID GAMMA-RAY REPEATERS; SOLID QUARK STARS; GIANT-FLARE; SGR 1806-20; NEUTRON-STARS; OSCILLATIONS; HYPERFLARE; DISTANCE; BURSTS; QPOS AB We have searched for gravitational waves (GWs) associated with the SGR 1806-20 hyperflare of 27 December 2004. This event, originating from a Galactic neutron star, displayed exceptional energetics. Recent investigations of the x-ray light curve's pulsating tail revealed the presence of quasiperiodic oscillations (QPOs) in the 30-2000 Hz frequency range, most of which coincides with the bandwidth of the LIGO detectors. These QPOs, with well-characterized frequencies, can plausibly be attributed to seismic modes of the neutron star which could emit GWs. Our search targeted potential quasimonochromatic GWs lasting for tens of seconds and emitted at the QPO frequencies. We have observed no candidate signals above a predetermined threshold, and our lowest upper limit was set by the 92.5 Hz QPO observed in the interval from 150 s to 260 s after the start of the flare. This bound corresponds to a (90% confidence) root-sum-squared amplitude h(rss-det)(90%)=4.5x10(-22) strain Hz(-1/2) on the GW waveform strength in the detectable polarization state reaching our Hanford (WA) 4 km detector. We illustrate the astrophysical significance of the result via an estimated characteristic energy in GW emission that we would expect to be able to detect. The above result corresponds to 7.7x10(46) erg (=4.3x10(-8) Mc(2)), which is of the same order as the total (isotropic) energy emitted in the electromagnetic spectrum. This result provides a means to probe the energy reservoir of the source with the best upper limit on the GW waveform strength published and represents the first broadband asteroseismology measurement using a GW detector. C1 Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. Andrews Univ, Berrien Springs, MI 49104 USA. Australian Natl Univ, Canberra, ACT 0200, Australia. CALTECH, Pasadena, CA 91125 USA. CALTECH, CaRT, Pasadena, CA 91125 USA. Cardiff Univ, Cardiff CF2 3YB, S Glam, Wales. Carleton Coll, Northfield, MN 55057 USA. Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. Columbia Univ, New York, NY 10027 USA. Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. Hobart & William Smith Coll, Geneva, NY 14456 USA. Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. CALTECH, LIGO, Pasadena, CA 91125 USA. LIGO Hanford Observ, Richland, WA 99352 USA. LIGO Livingston Observ, Livingston, LA 70754 USA. MIT, LIGO, Cambridge, MA 02139 USA. Louisiana State Univ, Baton Rouge, LA 70803 USA. Louisiana Tech Univ, Ruston, LA 71272 USA. Loyola Univ, New Orleans, LA 70118 USA. Moscow MV Lomonosov State Univ, Moscow 119992, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Astron Observ, Tokyo 1818588, Japan. Northwestern Univ, Evanston, IL 60208 USA. Rochester Inst Technol, Rochester, NY 14623 USA. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. San Jose State Univ, San Jose, CA 95192 USA. SE Louisiana Univ, Hammond, LA 70402 USA. So Univ, Baton Rouge, LA 70813 USA. A&M Coll, Baton Rouge, LA 70813 USA. Stanford Univ, Stanford, CA 94305 USA. Syracuse Univ, Syracuse, NY 13244 USA. Penn State Univ, University Pk, PA 16802 USA. Univ Texas, Brownsville, TX 78520 USA. Texas Southmost Coll, Brownsville, TX 78520 USA. Trinity Univ, San Antonio, TX 78212 USA. Univ Illes Balears, E-07122 Palma de Mallorca, Spain. Leibniz Univ Hannover, D-30167 Hannover, Germany. Univ Adelaide, Adelaide, SA 5005, Australia. Univ Birmingham, Birmingham B15 2TT, W Midlands, England. Univ Florida, Gainesville, FL 32611 USA. Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. Univ Maryland, College Pk, MD 20742 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Univ Oregon, Eugene, OR 97403 USA. Univ Rochester, Rochester, NY 14627 USA. Univ Salerno, I-84084 Fisciano, Salerno, Italy. Univ Sannio, I-82100 Benevento, Italy. Univ Southampton, Southampton SO17 1BJ, Hants, England. Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. Univ Washington, Seattle, WA 98195 USA. Univ Western Australia, Crawley, WA 6009, Australia. Univ Wisconsin, Milwaukee, WI 53201 USA. Washington State Univ, Pullman, WA 99164 USA. RP Abbott, B (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. RI Frey, Raymond/E-2830-2016; Howell, Eric/H-5072-2014; Ward, Robert/I-8032-2014; Vyatchanin, Sergey/J-2238-2012; Khalili, Farit/D-8113-2012; Chiadini, Francesco/E-1812-2015; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Messaritaki, Eirini/D-7393-2016; Tarallo, Marco/B-2096-2012; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Chow, Jong/A-3183-2008; Kawabe, Keita/G-9840-2011; Finn, Lee Samuel/A-3452-2009; Agresti, Juri/G-8168-2012; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013; Schutz, Bernard/B-1504-2010; zhao, chunnong/A-1373-2008; Freise, Andreas/F-8892-2011; Barriga, Pablo/A-3929-2008; Lam, Ping Koy/A-5276-2008; Galdi, Vincenzo/B-1670-2008; McClelland, David/E-6765-2010; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010; Casey, Morag/C-9703-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; OI Stuver, Amber/0000-0003-0324-5735; Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Aulbert, Carsten/0000-0002-1481-8319; Frey, Raymond/0000-0003-0341-2636; Howell, Eric/0000-0001-7891-2817; LONGO, Maurizio/0000-0001-8325-4003; Pierro, Vincenzo/0000-0002-6020-5521; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Pinto, Innocenzo M./0000-0002-2679-4457; Chiadini, Francesco/0000-0002-9339-8622; Vecchio, Alberto/0000-0002-6254-1617; Postiglione, Fabio/0000-0003-0628-3796; Tarallo, Marco/0000-0001-5169-4987; Sigg, Daniel/0000-0003-4606-6526; Chow, Jong/0000-0002-2414-5402; Finn, Lee Samuel/0000-0002-3937-0688; Agresti, Juri/0000-0001-6119-2470; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Lam, Ping Koy/0000-0002-4421-601X; Galdi, Vincenzo/0000-0002-4796-3600; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846; Freise, Andreas/0000-0001-6586-9901; MATTA, VINCENZO/0000-0002-2046-4027; MARANO, Stefano/0000-0002-5307-0980; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Papa, M.Alessandra/0000-0002-1007-5298 NR 32 TC 45 Z9 45 U1 2 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD SEP PY 2007 VL 76 IS 6 AR 062003 DI 10.1103/PhysRevD.76.062003 PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 215CW UT WOS:000249786900012 ER PT J AU Hickel, S Adams, NA Mansour, NN AF Hickel, S. Adams, N. A. Mansour, N. N. TI Implicit subgrid-scale modeling for large-eddy simulation of passive-scalar mixing SO PHYSICS OF FLUIDS LA English DT Article ID QUANTITIES LIKE TEMPERATURE; TURBULENT CHANNEL FLOW; NUMERICAL ERRORS; MASS-TRANSFER; NUMBER; WALL; DECONVOLUTION; CONDUCTIVITY; TRANSPORT; SCHEMES AB Further development of large-eddy simulation (LES) faces as major obstacles the strong coupling between subgrid-scale (SGS) modeling and the truncation error of the numerical discretization. One can exploit this link by developing discretization methods where the truncation error itself functions as an implicit SGS model. The name "implicit LES" is used for approaches that merge the SGS model and numerical discretization. In this paper, the implicit SGS modeling environment provided by the adaptive local deconvolution method is extended to LES of passive-scalar mixing. The resulting adaptive advection algorithm is discussed with respect to its numerical and turbulence-theoretical background. We demonstrate that the new method allows for reliable predictions of the turbulent transport of passive scalars in isotropic turbulence and in turbulent channel flow for a wide range of Schmidt numbers. (c) 2007 American Institute of Physics. C1 Tech Univ Munich, Inst Aerodynam, D-85747 Garching, Germany. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hickel, S (reprint author), Tech Univ Munich, Inst Aerodynam, D-85747 Garching, Germany. EM sh@tum.de RI Hickel, Stefan/H-4022-2011; Adams, Nikolaus/H-7247-2014 OI Hickel, Stefan/0000-0002-7463-9531; Adams, Nikolaus/0000-0001-5048-8639 NR 41 TC 26 Z9 26 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD SEP PY 2007 VL 19 IS 9 AR 095102 DI 10.1063/1.2770522 PG 13 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 215DC UT WOS:000249787500037 ER PT J AU Delcourt, DC Leblanc, F Seki, K Terada, N Moore, TE Fok, MC AF Delcourt, D. C. Leblanc, F. Seki, K. Terada, N. Moore, T. E. Fok, M. -C. TI Ion energization during substorms at Mercury SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Session on Relation between Exosphere-Magnetosphere-Surface on Mercury and the Moon CY 2006 CL Vienna, AUSTRIA SP European Geosci Union DE Mercury's magnetosphere; charged particle motion and acceleration; substorms ID FIELD; MAGNETOSPHERE; MAGNETOTAIL; EXOSPHERE; DYNAMICS; MODEL AB We investigate the dynamics of magnetospheric ions during transient reconfigurations of Mercury's magnetotail. At Earth, numerous observations during similar events reveal a prominent energization (up to the hundreds of keV range) of heavy ions (O+) originating from the topside ionosphere. This energization likely results from a resonant nonadiabatic interaction with the electric field that is induced by dipolarization of the magnetic field lines, the time scale of this reconfiguration being comparable to the heavy ion cyclotron period. The question then arises whether such an energization may occur at Mercury. Using single-particle simulations in time-varying electric and magnetic fields, we show that prominent nonadiabatic heating is obtained for ions with small mass-to-charge ratios (e.g., H+, He+). As for heavy ions (e.g., Na+, Ca+) that have cyclotron periods well above the time scale of the magnetotail reconfiguration (several seconds), a weaker energization is obtained. The resonant heating mechanism that we examine here may be of importance for solar wind protons that gain access to the inner hermean magnetotail as well as for light ions of planetary origin that directly feed the near-Mercury plasma sheet. (C) 2007 Elsevier Ltd. All rights reserved. C1 IPSL, CNRS, CETP, St Maur des Fosses, France. IPSL, CNRS, Serv Aeron, Verrieres Le Buisson, France. Nagoya Univ, STEL, Nagoya, Aichi, Japan. NIICT, Tokyo, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Delcourt, DC (reprint author), IPSL, CNRS, CETP, St Maur des Fosses, France. EM dominique.delcourt@cetp.ipsl.fr RI Moore, Thomas/D-4675-2012; Fok, Mei-Ching/D-1626-2012 OI Moore, Thomas/0000-0002-3150-1137; NR 27 TC 10 Z9 10 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD SEP PY 2007 VL 55 IS 11 BP 1502 EP 1508 DI 10.1016/j.pss.2006.11.026 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232VJ UT WOS:000251048000003 ER PT J AU Krishna, S Gunapala, SD Bandara, SV Hill, C Ting, DZ AF Krishna, Sanjay Gunapala, Sarath D. Bandara, Sumith V. Hill, Cory Ting, David Z. TI Quantum dot based infrared focal plane Arrays SO PROCEEDINGS OF THE IEEE LA English DT Article DE focal plane arrays; infrared detectors; nanoscale; quantum dots; self-assembly ID A-WELL DETECTOR; TEMPERATURE OPERATION; PHOTODETECTORS; ABSORPTION AB In the past decade, there has been active research on infrared detectors based on intersubband transitions in self-assembled quantum dots (QDs). In the past two years, at least four research groups have independently demonstrated focal plane arrays based on this technology. in this paper, the. progress from the first raster scanned image obtained with a QD detector to the demonstration of a 640 x 512 imager based on self-assembled QDs is reviewed. in particular, emphasis will be placed on a novel quantum clots-in-a-well (DWELL) design, which represents a hybrid between a conventional quantum-well infrared photodetector (QWIP) and a quantum-dot infrared photodetector (QDIP). In the DWELL detectors, the active region consists of InAs quantum dots embedded in an InGaAs quantum well. Like QDIPs, the DWELL detectors. have 3-D confinement and display normal incidence operation while demonstrating reproducible "dial-in recipes" for control over the operating wavelength, like QWIPs. Moreover, the DWELL detectors also have demonstrated bias-tunability and multi-color operation in the midwave infrared (MWIR, 3-5 mu m), long-wave infrared (LWIR, 8-12 mu m), and very long wave infrared (VLWIR, > 14 mu m) regimes. Recently midformat 320 x 256 and 640 x 512 focal plane arrays (FPAs) with an NETD of 40 mK at T = 60 K have been reported. The paper will conclude with a perspective on the future directions on the research on QDIP FPA including enhanced functionality and higher operating temperatures. C1 Univ New Mexico, Ctr High Technol Mat, Dept Elect & Comp Engn, Albuquerque, NM 87106 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP Krishna, S (reprint author), Univ New Mexico, Ctr High Technol Mat, Dept Elect & Comp Engn, Albuquerque, NM 87106 USA. EM skrishna@chtm.unm.edu; Sarath.D.Gunapala@jpl.nasa.gov RI Krishna, Sanjay /C-5766-2009 NR 37 TC 32 Z9 32 U1 2 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9219 J9 P IEEE JI Proc. IEEE PD SEP PY 2007 VL 95 IS 9 BP 1838 EP 1852 DI 10.1109/JPROC.2007.900969 PG 15 WC Engineering, Electrical & Electronic SC Engineering GA 230DT UT WOS:000250856800012 ER PT J AU Barnes, JW AF Barnes, Jason W. TI Effects of orbital eccentricity on extrasolar planet transit detectability and light curves SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID TERRESTRIAL PLANETS; HD 209458B; PARAMETERS; ROTATION; OBLATENESS; MISSION AB It is shown herein that planets with eccentric orbits are more likely to transit than circularly orbiting planets with the same semimajor axis by a factor of (1-e(2))(-1). If the orbital parameters of discovered transiting planets are known, as from follow-up radial velocity observations, then the transit-detected planet population is easily debiased of this effect. The duration of a planet's transit depends on its eccentricity and longitude of periastron; transits near periastron are shorter, and those near apoastron last longer, for a given impact parameter. If fitting for the stellar radius with the other transit parameters, this effect causes a systematic error in the resulting measurements. If the stellar radius is instead held fixed at a value measured independently, then it is possible to place a lower limit on the planet's eccentricity using photometry alone. Orbital accelerations cause a difference in the planet's ingress and egress durations that lead to an asymmetry in the transit light curve that could be used along with the transit velocity measurement to uniquely measure the planet's eccentricity and longitude of periapsis. However, the effect is too small to be measured with current technology. The habitability of transiting terrestrial planets found by Kepler depends on those planets' orbital eccentricities. While Kepler will be able to place lower limits on those planets' orbital eccentricity, the actual value for any given planet will likely remain unknown. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Barnes, JW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jason@barnesos.net RI Barnes, Jason/B-1284-2009 OI Barnes, Jason/0000-0002-7755-3530 NR 22 TC 60 Z9 60 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2007 VL 119 IS 859 BP 986 EP 993 DI 10.1086/522039 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 221LJ UT WOS:000250228500004 ER PT J AU Engelbracht, CW Blaylock, M Su, KYL Rho, J Rieke, GH Muzerolle, J Padgett, DL Hines, DC Gordon, KD Fadda, D Noriega-Crespo, A Kelly, DM Latter, WB Hinz, JL Misselt, KA Morrison, JE Stansberry, JA Shupe, DL Stolovy, S Wheaton, WA Young, ET Neugebauer, G Wachter, S Perez-Gonzalez, PG Frayer, DT Marleau, FR AF Engelbracht, C. W. Blaylock, M. Su, K. Y. L. Rho, J. Rieke, G. H. Muzerolle, J. Padgett, D. L. Hines, D. C. Gordon, K. D. Fadda, D. Noriega-Crespo, A. Kelly, D. M. Latter, W. B. Hinz, J. L. Misselt, K. A. Morrison, J. E. Stansberry, J. A. Shupe, D. L. Stolovy, S. Wheaton, Wm. A. Young, E. T. Neugebauer, G. Wachter, S. Perez-Gonzalez, P. G. Frayer, D. T. Marleau, F. R. TI Absolute calibration and characterization of the multiband imaging photometer for spitzer. I. The stellar calibrator sample and the 24 mu m calibration SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SPECTRAL IRRADIANCE CALIBRATION; MIDCOURSE-SPACE-EXPERIMENT; INFRARED ARRAY CAMERA; NEARBY GALAXIES; TELESCOPE; REDUCTION; EVOLUTION; ISOPHOT; STARS; 2MASS AB We present the stellar calibrator sample and the conversion from instrumental to physical units for the 24 mm channel of the Multiband Imaging Photometer for Spitzer (MIPS). The primary calibrators are A stars, and the calibration factor based on those stars is 4.54 x 10(-2) MJy sr(-1) (DN s(-1))(-1), with a nominal uncertainty of 2%. We discuss the data reduction procedures required to attain this accuracy; without these procedures, the calibration factor obtained using the automated pipeline at the Spitzer Science Center is lower. We 1.6% +/- 0.6% extend this work to predict 24 mu m flux densities for a sample of 238 stars that covers a larger range of flux densities and spectral types. We present a total of 348 measurements of 141 stars at 24 mm. This sample covers a factor of similar to 460 in 24 mm flux density, from 8.6 mJy up to 4.0 Jy. We show that the calibration is linear over that range with respect to target flux and background level. The calibration is based on observations made using 3 s exposures; a preliminary analysis shows that the calibration factor may be 1% and 2% lower for 10 and 30 s exposures, respectively. We also demonstrate that the calibration is very stable: over the course of the mission, repeated measurements of our routine calibrator, HD 159330, show a rms scatter of only 0.4%. Finally, we show that the point-spread function (PSF) is well measured and allows us to calibrate extended sources accurately; Infrared Astronomy Satellite (IRAS) and MIPS measurements of a sample of nearby galaxies are identical within the uncertainties. C1 Univ Arizona, Steward Observat, Tucson, AZ 85721 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Space Sci Inst, Boulder, CO USA. CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. Univ Complutense Madrid, Fac CC Fis, Dept Astronfis, E-28040 Madrid, Spain. RP Engelbracht, CW (reprint author), Univ Arizona, Steward Observat, Tucson, AZ 85721 USA. EM cengelbracht@as.arizona.edu; mblaylock@as.arizona.edu; ksu@as.arizona.edu; rho@ipac.caltech.edu; grieke@as.arizona.edu; jmuzerolle@as.arizona.edu; dlp@ipac.caltech.edu; dhines@as.arizona.edu; kgordon@as.arizona.edu; fadda@ipac.caltech.edu; alberto@ipac.caltech.edu; dkelly@as.arizona.edu; latter@ipac.caltech.edu; jhinz@as.arizona.edu; kmisselt@as.arizona.edu; jmorrison@as.arizona.edu; jstansberry@as.arizona.edu; shupe@ipac.caltech.edu; stolovy@ipac.caltech.edu; waw@ipac.caltech.edu; eyoung@as.arizona.edu; gxn@as.arizona.edu; wachter@ipac.caltech.edu; pgperez@as.arizona.edu; frayer@ipac.caltech.edu; marleau@ipac.caltech.edu RI Perez-Gonzalez, Pablo/J-2871-2016 OI Perez-Gonzalez, Pablo/0000-0003-4528-5639 NR 36 TC 209 Z9 209 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2007 VL 119 IS 859 BP 994 EP 1018 DI 10.1086/521881 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 221LJ UT WOS:000250228500005 ER PT J AU Gordon, KD Engelbracht, CW Fadda, D Stansberry, J Wachter, S Frayer, DT Rieke, G Noriega-Crespo, A Latter, WB Young, E Neugebauer, G Balog, Z Beeman, JW Dole, H Egami, E Haller, EE Hines, D Kelly, D Marleau, F Misselt, K Morrison, J Perez-Gonzalez, P Rho, J Wheaton, WA AF Gordon, Karl D. Engelbracht, Charles W. Fadda, Dario Stansberry, John Wachter, Stefanie Frayer, Dave T. Rieke, George Noriega-Crespo, Alberto Latter, William B. Young, Erick Neugebauer, Gerry Balog, Zoltan Beeman, Jeffrey W. Dole, Herve Egami, Eiichi Haller, Eugene E. Hines, Dean Kelly, Doug Marleau, Francine Misselt, Karl Morrison, Jane Perez-Gonzalez, Pablo Rho, Jeonghee Wheaton, Wm. A. TI Absolute calibration and characterization of the multiband imaging photometer for spitzer. II. 70 mu m imaging SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID NEARBY GALAXIES; SOURCE COUNTS; EVOLUTION; SIRTF; STAR; MIPS; VIEW AB The absolute calibration and characterization of the Multiband Imaging Photometer for Spitzer (MIPS) 70 mu m coarse- and fine-scale imaging modes are presented based on over 2.5 yr of observations. Accurate photometry ( especially for faint sources) requires two simple processing steps beyond the standard data reduction to remove long-term detector transients. Point-spread function (PSF) fitting photometry is found to give more accurate flux densities than aperture photometry. Based on the PSF fitting photometry, the calibration factor shows no strong trend with flux density, background, spectral type, exposure time, or time since anneals. The coarse- scale calibration sample includes observations of stars with flux densities from 22 mJy to 17 Jy, on backgrounds from 4 to 26 MJy sr(-1), and with spectral types from B to M. The coarse- scale calibration is 702 +/- 35 MJy sr(-1) MIPS70(-1) (5% uncertainty) and is based on measurements of 66 stars. The instrumental units of the MIPS 70 mm coarse- and fine-scale imaging modes are called MIPS70 and MIPS70F, respectively. The photometric repeatability is calculated to be 4.5% from two stars measured during every MIPS campaign and includes variations on all timescales probed. The preliminary fine-scale calibration factor is 2894 +/- 294 MJy sr(-1) MIPS70F(-1) (10% uncertainty) based on 10 stars. The uncertainties in the coarse- and fine-scale calibration factors are dominated by the 4.5% photometric repeatability and the small sample size, respectively. The 5 sigma, 500 s sensitivity of the coarse- scale observations is 6-8 mJy. This work shows that the 5 sigma MIPS 70 mm array produces accurate, well-calibrated photometry and validates the MIPS 70 mu m operating strategy, especially the use of frequent stimulator flashes to track the changing responsivities of the Ge:Ga detectors. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. Lawrence Berkey Natl Lab, Mat Sci Div, Berkeley, CA USA. Inst Astronphys Spatiale, Orsay, France. Univ Calif Berkeley, Dept Mat Sci & Engn, Berkeley, CA USA. Space Sci Inst, Boulder, CO USA. Univ Complutense Madrid, Fac CC Fis, Dept Astronfis, Madrid, Spain. RP Gordon, KD (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RI Perez-Gonzalez, Pablo/J-2871-2016 OI Perez-Gonzalez, Pablo/0000-0003-4528-5639 NR 31 TC 152 Z9 152 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2007 VL 119 IS 859 BP 1019 EP 1037 DI 10.1086/522675 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 221LJ UT WOS:000250228500006 ER PT J AU Antcliff, RR AF Antcliff, Richard R. TI Three tsunamis cresting move R&D lab of the future SO RESEARCH-TECHNOLOGY MANAGEMENT LA English DT Editorial Material C1 NASA, Langley Res Ctr, Adv Planning & Partnership Off, Hampton, VA 23665 USA. RP Antcliff, RR (reprint author), NASA, Langley Res Ctr, Adv Planning & Partnership Off, Hampton, VA 23665 USA. EM Richard.R.Antcliff@nasa.gov NR 0 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 J9 RES TECHNOL MANAGE JI Res.-Technol. Manage. PD SEP-OCT PY 2007 VL 50 IS 5 BP 2 EP 3 PG 2 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA 204YI UT WOS:000249079500001 ER PT J AU Polk, JE Marrese-Reading, CM Thornber, B Dang, L Johnson, LK Katz, I AF Polk, J. E. Marrese-Reading, C. M. Thornber, B. Dang, L. Johnson, L. K. Katz, I. TI Scanning optical pyrometer for measuring temperatures in hollow cathodes SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article AB Life-limiting processes in hollow cathodes are determined largely by the temperature of the electron emitter. To support cathode life assessment, a noncontact temperature measurement technique which employs a stepper motor-driven fiber optic probe was developed. The probe is driven inside the hollow cathode and collects light radiated by the hot interior surface of the emitter. Ratio pyrometry is used to determine the axial temperature profile. Thermocouples on the orifice plate provide measurements of the external temperature during cathode operation and are used to calibrate the pyrometer system in situ with a small oven enclosing the externally heated cathode. The diagnostic method and initial measurements of the temperature distribution in a hollow cathode are discussed. (c) 2007 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Int Space Univ, F-67000 Strasbourg, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Polk, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Thornber, Ben/0000-0002-7665-089X NR 16 TC 7 Z9 7 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 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD SEP PY 2007 VL 78 IS 9 AR 093101 DI 10.1063/1.2774828 PG 8 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 215DF UT WOS:000249787800002 PM 17902941 ER PT J AU Elvidge, CD Tuttle, BT Sutton, PS Baugh, KE Howard, AT Milesi, C Bhaduri, BL Nemani, R AF Elvidge, Christopher D. Tuttle, Benjamin T. Sutton, Paul S. Baugh, Kimberly E. Howard, Ara T. Milesi, Cristina Bhaduri, Budhendra L. Nemani, Ramakrishna TI Global distribution and density of constructed impervious surfaces SO SENSORS LA English DT Article DE impervious surfaces; constructed area; urbanization; nighttime lights; population grid; ISA ID UNITED-STATES; COVER; IMAGERY; LIGHTS; SYSTEM; AREA AB We present the first global inventory of the spatial distribution and density of constructed impervious surface area (ISA). Examples of ISA include roads, parking lots, buildings, driveways, sidewalks and other manmade surfaces. While high spatial resolution is required to observe these features, the new product reports the estimated density of ISA on a one-km(2) grid based on two coarse resolution indicators of ISA-the brightness of satellite observed nighttime lights and population count. The model was calibrated using 30-meter resolution ISA of the USA from the U. S. Geological Survey. Nominally the product is for the years 2000-01 since both the nighttime lights and reference data are from those two years. We found that 1.05% of the United States land area is impervious surface ( 83,337 km(2)) and 0.43% of the world's land surface ( 579,703 km(2)) is constructed impervious surface. China has more ISA than any other country ( 87,182 km2), but has only 67 m(2) of ISA per person, compared to 297 m(2) per person in the USA. The distribution of ISA in the world's primary drainage basins indicates that watersheds damaged by ISA are primarily concentrated in the USA, Europe, Japan, China and India. The authors believe the next step for improving the product is to include reference ISA data from many more areas around the world. C1 NOAA, Natl Geophys Data Ctr, Earth Observat Grp, Boulder, CO 80305 USA. Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. Univ Denver, Dept Geog, Denver, CO USA. Fdn Calif State Univ, Monterey, CA USA. Oak Ridge Natl Lab, US Dept Energy, Oak Ridge, TN USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Elvidge, CD (reprint author), NOAA, Natl Geophys Data Ctr, Earth Observat Grp, 325 Broadway, Boulder, CO 80305 USA. EM chris.elvidge@noaa.gov; ben.tuttle@noaa.gov; psutton@du.edu; kim.baugh@noaa.gov; ara.t.howard@noaa.gov; cristina.milesi@gmail.com; bhaduribl@ornl.gov; rnemani@arc.nasa.gov RI Elvidge, Christopher/C-3012-2009; Sutton, Paul/A-6764-2013 OI Sutton, Paul/0000-0001-6972-3256 NR 28 TC 146 Z9 162 U1 4 U2 53 PU MOLECULAR DIVERSITY PRESERVATION INT PI BASEL PA MATTHAEUSSTRASSE 11, CH-4057 BASEL, SWITZERLAND SN 1424-8220 J9 SENSORS-BASEL JI Sensors PD SEP PY 2007 VL 7 IS 9 BP 1962 EP 1979 DI 10.3390/s7091962 PG 18 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA 214GH UT WOS:000249723500020 ER PT J AU Grubler, A Nakicenovic, N Riahi, K Wagner, F Fischer, G Keppo, I Obersteiner, M O'Neill, B Rao, S Tubiello, F AF Gruebler, Arnulf Nakicenovic, Nebojsa Riahi, Keywan Wagner, Fabian Fischer, Guenther Keppo, Ilkka Obersteiner, Michael O'Neill, Brian Rao, Shilpa Tubiello, Francesco TI Integrated assessment of uncertainties in greenhouse gas emissions and their mitigation: Introduction and overview SO TECHNOLOGICAL FORECASTING AND SOCIAL CHANGE LA English DT Editorial Material AB This paper provides the background and the context for the analyses presented in the seven papers of this Special Issue on Integrated Assessment of Uncertainties in Greenhouse Gas Emissions and their Mitigation. First, the main topic and content of the Special Issue is given, followed by an overall overview. Second, detailed overviews and summaries of the seven papers are given. The specific analytical and methodological features and findings of each paper are highlighted and the linkages between the various papers presented in the Special Issue are provided. (c) 2006 Elsevier Inc. All rights reserved. C1 Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria. Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. Vienna Univ Technol, Dept Power Syst & Energy Econ, Vienna, Austria. Brown Univ, Watson Inst Int Studies, Providence, RI 02912 USA. Columbia Univ, Goddard Inst Space Studies, New York, NY USA. RP Grubler, A (reprint author), Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria. EM gruebler@iiasa.ac.at RI Riahi, Keywan/B-6426-2011; O'Neill, Brian/E-6531-2013; OI Riahi, Keywan/0000-0001-7193-3498; Grubler, Arnulf/0000-0002-6225-7712 NR 0 TC 12 Z9 12 U1 1 U2 8 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0040-1625 J9 TECHNOL FORECAST SOC JI Technol. Forecast. Soc. Chang. PD SEP PY 2007 VL 74 IS 7 BP 873 EP 886 DI 10.1016/j.techfore.2006.07.009 PG 14 WC Business; Planning & Development SC Business & Economics; Public Administration GA 211HP UT WOS:000249515200001 ER PT J AU Tubiello, FN Fischer, GI AF Tubiello, Francesco N. Fischer, Guenther TI Reducing climate change impacts on agriculture: Global and regional effects of mitigation, 2000-2080 SO TECHNOLOGICAL FORECASTING AND SOCIAL CHANGE LA English DT Article DE agriculture; climate impacts; mitigation; world food supply ID AIR CO2 ENRICHMENT; ELEVATED CO2; RESPONSES; CROPS; RISK AB What are the implications for agriculture of mitigating greenhouse gas emissions? By when and by how much are impacts reduced? Where does it matter most? We investigated these questions within the new A2 emission scenario, recently developed at the International Institute of Applied Systems Analysis with revised population and gross domestic product projections. Coupling an agro-ecological model to a global food trade model, two distinct sets of climate simulations were analyzed: 1) A non-mitigated scenario, with atmospheric CO2 concentrations over 800 ppm by 2 100; and 2) A mitigation scenario, with CO2 Concentrations stabilized at 5 50 ppm by 2100. Impacts of climate change on crop yield were evaluated for the period 1990-2080, then used as input for economic analyses. Key trends were computed over the 21st century for food demand, production and trade, focusing on potential monetary (aggregate value added) and human (risk of hunger) impacts. The results from this study suggested that mitigation could positively impact agriculture. With mitigation, global costs of climate change, though relatively small in absolute amounts, were reduced by 75-100%; and the number of additional people at risk of malnutrition was reduced by 80-95%. Significant geographic and temporal differences were found. Regional effects often diverged from global net results, with some regions worse off under mitigation compared to the unmitigated case. (c) 2006 Elsevier Inc. All rights reserved. C1 Int Inst Appl Syst Anal, Land Use Change & Agr Program, A-2361 Laxenburg, Austria. Columbia Univ, Goddard Inst Space Studies, New York, NY USA. RP Tubiello, FN (reprint author), Int Inst Appl Syst Anal, Land Use Change & Agr Program, A-2361 Laxenburg, Austria. EM franci@giss.nasa.gov RI zhong, honglin/C-2633-2012 NR 33 TC 77 Z9 83 U1 5 U2 38 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0040-1625 J9 TECHNOL FORECAST SOC JI Technol. Forecast. Soc. Chang. PD SEP PY 2007 VL 74 IS 7 BP 1030 EP 1056 DI 10.1016/j.techfore.2006.05.027 PG 27 WC Business; Planning & Development SC Business & Economics; Public Administration GA 211HP UT WOS:000249515200006 ER PT J AU Fischer, G Tubiello, FN Van Velthuizen, H Wiberg, DA AF Fischer, Guenther Tubiello, Francesco N. Van Velthuizen, Harrij Wiberg, David A. TI Climate change impacts on irrigation water requirements: Effects of mitigation, 1990-2080 SO TECHNOLOGICAL FORECASTING AND SOCIAL CHANGE LA English DT Article DE water; agriculture; irrigation; climate change; mitigation ID SOCIOECONOMIC SCENARIOS; INTEGRATED ASSESSMENT; SRES EMISSIONS; RESOURCES AB Potential changes in global and regional agricultural water demand for irrigation were investigated within a new socio-economic scenario, A2r, developed at the International Institute for Applied Systems Analysis (IIASA) with and without climate change, with and without mitigation of greenhouse gas emissions. Water deficits of crops were developed with the Food and Agriculture Organization (FAO)-IIASA Agro-ecological Zone model, based on daily water balances at 0.5 degrees latitude x 0.5 degrees longitude and then aggregated to regions and the globe. Future regional and global irrigation water requirements were computed as a function of both projected irrigated land and climate change and simulations were performed from 1990 to 2080. Future trends for extents of irrigated land, irrigation water use, and withdrawals were computed, with specific attention given to the implications of climate change mitigation. Renewable water-resource availability was estimated under current and future climate conditions. Results suggest that mitigation of climate change may have significant positive effects compared with unmitigated climate change. Specifically, mitigation reduced the impacts of climate change on agricultural water requirements by about 40%, or 125-160billion m(3) (Gm(3)) compared with unmitigated climate. Simple estimates of future changes in irrigation efficiency and water costs suggest that by 2080 mitigation may translate into annual cost reductions of about 10billion US$. (c) 2006 Elsevier Inc. All rights reserved. C1 Int Inst Appl Syst Anal, Land Use Change & Agr Program, A-2361 Laxenburg, Austria. Columbia Univ, Goddard Inst Space Studies, New York, NY USA. RP Fischer, GI (reprint author), Int Inst Appl Syst Anal, Land Use Change & Agr Program, A-2361 Laxenburg, Austria. EM fisher@iiasa.ac.at; franci@giss.nasa.gov; velt@iiasa.ac.at OI Wiberg, David/0000-0001-9515-1538 NR 31 TC 144 Z9 153 U1 4 U2 52 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0040-1625 J9 TECHNOL FORECAST SOC JI Technol. Forecast. Soc. Chang. PD SEP PY 2007 VL 74 IS 7 BP 1083 EP 1107 DI 10.1016/j.techfore.2006.05.021 PG 25 WC Business; Planning & Development SC Business & Economics; Public Administration GA 211HP UT WOS:000249515200008 ER PT J AU Charlson, RJ Ackerman, AS Bender, FAM Anderson, TL Liu, Z AF Charlson, Robert J. Ackerman, Andrew S. Bender, Frida A-M. Anderson, Theodore L. Liu, Zhaoyan TI On the climate forcing consequences of the albedo continuum between cloudy and clear air SO TELLUS SERIES B-CHEMICAL AND PHYSICAL METEOROLOGY LA English DT Article ID RADIANT ENERGY SYSTEM; ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; LARGE-EDDY SIMULATIONS; BOUNDARY-LAYER CLOUDS; TRADE-WIND CUMULI; SATELLITE DATA; RAMAN LIDAR; PART I; AEROSOL AB It has been long understood that the partly cloudy atmosphere manifests a continuum of states between the end members 'clear' and 'cloud.' Nevertheless, many research methods are premised on a dichotomy of states-for example, those that use 'cloud cover' or 'cloud-clearing.' Here we consider the consequences of this practice for studies of aerosol-climate effects. Aerosols affect the Earth's energy budget primarily by affecting albedo; therefore, we explore the nature of albedo variability in the partly cloudy marine boundary layer on scales down to a few tens of metres. We employ two diagnostic tools: a cloud resolving model and an albedo proxy derived from high altitude lidars. We show that a continuum of albedo values results from indeterminate and variable combinations of hydrated aerosol and wispy (including subvisible) clouds. Two consequences arise. First, cloud-clearing schemes employed by different observational methods are mutually inconsistent and are sensitive to concentrations of unactivated aerosol particles. Second, aerosol radiative forcing (the sensitivity of overall albedo to changes in aerosol concentration) is inaccurately calculated as the average of clear and overcast conditions. Together, these results imply that dividing the aerosol forcing problem into 'direct' and 'indirect' components may lead to substantial errors. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. Univ Stockholm, Dept Meteorol, S-10691 Stockholm, Sweden. Natl Inst Aerosp, Hampton, VA 23666 USA. RP Ackerman, AS (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM andrew.ackerman@nasa.gov RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Ackerman, Andrew/D-4433-2012; Bender, Frida/D-6228-2012 OI Liu, Zhaoyan/0000-0003-4996-5738; Ackerman, Andrew/0000-0003-0254-6253; NR 48 TC 71 Z9 72 U1 0 U2 4 PU CO-ACTION PUBLISHING PI JARFALLA PA RIPVAGEN 7, JARFALLA, SE-175 64, SWEDEN SN 0280-6509 EI 1600-0889 J9 TELLUS B JI Tellus Ser. B-Chem. Phys. Meteorol. PD SEP PY 2007 VL 59 IS 4 BP 715 EP 727 DI 10.1111/j.1600-0889.2007.00297.x PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 206RH UT WOS:000249200100008 ER PT J AU Malik, MR Balakumar, P AF Malik, M. R. Balakumar, P. TI Acoustic receptivity of Mach 4.5 boundary layer with leading-edge bluntness SO THEORETICAL AND COMPUTATIONAL FLUID DYNAMICS LA English DT Article DE boundary layer; hypersonic; receptivity; stability; transition; bluntness ID FLAT-PLATE; DISTURBANCES; TRANSITION; STABILITY AB Boundary layer receptivity to two-dimensional slow and fast acoustic waves is investigated by solving Navier-Stokes equations for Mach 4.5 flow over a flat plate with a finite-thickness leading edge. Higher order spatial and temporal schemes are employed to obtain the solution whereby the flat-plate leading edge region is resolved by providing a sufficiently refined grid. The results show that the instability waves are generated in the leading edge region and that the boundary-layer is much more receptive to slow acoustic waves (by almost a factor of 20) as compared to the fast waves. Hence, this leading-edge receptivity mechanism is expected to be more relevant in the transition process for high Mach number flows where second mode instability is dominant. Computations are performed to investigate the effect of leading-edge thickness and it is found that bluntness tends to stabilize the boundary layer. Furthermore, the relative significance of fast acoustic waves is enhanced in the presence of bluntness. The effect of acoustic wave incidence angle is also studied and it is found that the receptivity of the boundary layer on the 'windward' side (with respect to the acoustic forcing) decreases by more than a factor of four when the incidence angle is increased from 0 degrees to 45 degrees. However, the receptivity coefficient for the 'leeward' side is found to vary relatively weakly with the incidence angle. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Malik, MR (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM mujeeb.r.malik@nasa.gov NR 20 TC 5 Z9 5 U1 0 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0935-4964 J9 THEOR COMP FLUID DYN JI Theor. Comput. Fluid Dyn. PD SEP PY 2007 VL 21 IS 5 BP 323 EP 342 DI 10.1007/s00162-007-0050-5 PG 20 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 198LM UT WOS:000248629600001 ER PT J AU Park, M Randel, WJ Gettelman, A Massie, ST Jiang, JH AF Park, Mijeong Randel, William J. Gettelman, Andrew Massie, Steven T. Jiang, Jonathan H. TI Transport above the Asian summer monsoon anticyclone inferred from Aura Microwave Limb Sounder tracers SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL TROPOPAUSE LAYER; LOWER STRATOSPHERE; WATER-VAPOR; LOWERMOST STRATOSPHERE; SEASONAL-VARIATION; EOS MLS; CONVECTION; MODEL; TROPOSPHERE; SATELLITE AB Tracer variability above the Asian summer monsoon anticyclone is investigated using Aura Microwave Limb Sounder (MLS) measurements of carbon monoxide, ozone, water vapor, and temperature during Northern Hemisphere summer ( June to August) of 2005. Observations show persistent maxima in carbon monoxide and minima in ozone within the anticyclone in the upper troposphere-lower stratosphere (UTLS) throughout summer, and variations in these tracers are closely related to the intensity of underlying deep convection. Temperatures in the UTLS are also closely coupled to deep convection ( cold anomalies are linked with enhanced convection), and the three-dimensional temperature patterns are consistent with a dynamical response to near-equatorial convection. Upper tropospheric water vapor in the monsoon region is strongly coherent with deep convection, both spatially and temporally. However, at the altitude of the tropopause, maximum water vapor is centered within the anticyclone, distant from the deepest convection, and is also less temporally correlated with convective intensity. Because the main outflow of deep convection occurs near similar to 12 km, well below the tropopause level ( similar to 16 km), we investigate the large-scale vertical transport within the anticyclone. The mean vertical circulation obtained from the ERA40 reanalysis data set and a free-running general circulation model is upward across the tropopause on the eastern end of the anticyclone, as part of the balanced three-dimensional monsoon circulation. In addition to deep transport from the most intense convection, this large-scale circulation may help explain the transport of constituents to tropopause level. C1 Natl Ctr Atmospher Res, Boulder, CO 80307 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Park, M (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM mijeong@ucar.edu RI Randel, William/K-3267-2016 OI Randel, William/0000-0002-5999-7162 NR 40 TC 115 Z9 124 U1 5 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 31 PY 2007 VL 112 IS D16 AR D16309 DI 10.1029/2006JD008294 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 208QX UT WOS:000249335400001 ER PT J AU Bibring, JP Arvidson, RE Gendrin, A Gondet, B Langevin, Y Le Mouelic, S Mangold, N Morris, RV Mustard, JF Poulet, F Quantin, C Sotin, C AF Bibring, J.-P. Arvidson, R. E. Gendrin, A. Gondet, B. Langevin, Y. Le Mouelic, S. Mangold, N. Morris, R. V. Mustard, J. F. Poulet, F. Quantin, C. Sotin, C. TI Coupled ferric oxides and sulfates on the Martian surface SO SCIENCE LA English DT Article ID MERIDIANI-PLANUM; BURNS FORMATION; REFLECTIVITY SPECTRA; TERRESTRIAL ANALOG; TERRA-MERIDIANI; MARS; HEMATITE; MINERALOGY; GOETHITE; SYSTEM AB The Mars Exploration Rover ( MER), Opportunity, showed that layered sulfate deposits in Meridiani Planum formed during a period of rising acidic ground water. Crystalline hematite spherules formed in the deposits as a consequence of aqueous alteration and were concentrated on the surface as a lag deposit as wind eroded the softer sulfate rocks. On the basis of Mars Express Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite ( OMEGA) orbital data, we demonstrate that crystalline hematite deposits are associated with layered sulfates in other areas on Mars, implying that Meridiani-like ground water systems were indeed widespread and representative of an extensive acid sulfate aqueous system. C1 Inst Astrophys Spatiale, F-91405 Orsay, France. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Univ Nantes, F-44322 Nantes, France. Interact & Dynam Environm Surface, F-91405 Orsay, France. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Brown Univ, Providence, RI 02912 USA. RP Bibring, JP (reprint author), Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France. EM bibring@ias.fr RI Quantin, Cathy/H-1516-2014 NR 29 TC 100 Z9 101 U1 3 U2 17 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD AUG 31 PY 2007 VL 317 IS 5842 BP 1206 EP 1210 DI 10.1126/science.1144174 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 205PJ UT WOS:000249126800036 PM 17673623 ER PT J AU Hurowitz, JA McLennan, SM AF Hurowitz, Joel A. McLennan, Scott M. TI A similar to 3.5 Ga record of water-limited, acidic weathering conditions on Mars SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE mars; weathering; rates; aluminum; clay; APXS ID X-RAY SPECTROMETER; PATHFINDER LANDING SITE; MERIDIANI-PLANUM; MOSSBAUER SPECTROMETER; CHEMICAL-COMPOSITION; DISSOLUTION RATES; SILICATE MINERALS; SPIRIT ROVER; GUSEV CRATER; ROCKS AB The secondary mineral budget on Earth is dominated by clay minerals, Al-hydroxides, and Fe-oxides, which are formed under the moderate pH, high water-to-rock ratio conditions typical of Earth's near-surface environment. In contrast, geochemical analyses of rocks and soils from landed missions to Mars indicate that secondary mineralogy is dominated by Mg (+/- Fe, Ca)-sulfates and Fe-oxides. This discrepancy can be explained as resulting from differences in the chemical weathering environment of Earth and Mars. We suggest that chemical weathering processes on Mars are dominated by: (1) a low-pH, sulfuric acid-rich environment in which the stoichiometric dissolution of labile mineral phases such as olivine and apatite ( +/- Fe-Ti oxides) is promoted; and (2) relatively low water-to-rock ratio, such that other silicate phases with slower dissolution rates (e.g., plagioclase, pyroxene) do not contribute substantially to the secondary mineral budget at the Martian surface. Under these conditions, Al-mobilization is limited, and the formation of significant Al-bearing secondary phases (e.g., clays, Al-hydroxides, Al-sulfates) is inhibited. The antiquity of rock samples analyzed in-situ on Mars suggest that water-limited acidic weathering conditions have more than likely been the defining characteristic of the Martian aqueous environment for billions of years. (C) 2007 Elsevier B.V. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. RP Hurowitz, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM joel.a.hurowitz@jpl.nasa.gov RI Hurowitz, Joel/A-8862-2008 NR 69 TC 81 Z9 82 U1 1 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD AUG 30 PY 2007 VL 260 IS 3-4 BP 432 EP 443 DI 10.1016/j.epsl.2007.05.043 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 206RK UT WOS:000249200400005 ER PT J AU Lee, MI Schubert, SD Suarez, MJ Bell, TL Kim, KM AF Lee, Myong-In Schubert, Siegfried D. Suarez, Max J. Bell, Thomas L. Kim, Kyu-Myong TI Diurnal cycle of precipitation in the NASA Seasonal to Interannual Prediction Project atmospheric general circulation model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CONTINENTAL UNITED-STATES; NORTH-AMERICAN MONSOON; MEASURING MISSION TRMM; TROPICAL PRECIPITATION; CLOUD ENSEMBLE; CLIMATE MODEL; GREAT-PLAINS; TOGA COARE; CONVECTION; RAINFALL AB [1] The global statistics of the diurnal cycle of warm-season precipitation simulated by NASA's Seasonal to Interannual Prediction Project (NASA/NSIPP) atmospheric general circulation model (AGCM) were evaluated using the Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) rain retrievals. The model has notable biases in the phase of the diurnal cycle over land, where it produces rainfall maxima in the early afternoon, several hours earlier than the observed evening maxima. The model also produces too little precipitation in the nighttime over land. Similar biases in the phase were found over ocean, although the statistics are less robust. An analysis of the convective and stratiform contributions to the precipitation indicates that the incorrect representation of the diurnal cycle is primarily tied to deficiencies in the deep convection scheme. A set of sensitivity experiments shows that the phase of the maximum diurnal precipitation is quite sensitive to the change of the convection starting (parcel origination) level and the increase of the convection adjustment (relaxation) timescale in the Relaxed Arakawa-Schubert scheme. Both modifications act to delay the timing for the maximum development of CAPE, which lead to improvements in the diurnal cycle of precipitation, especially in correcting the phase errors over land, although the modifications tend to reduce the diurnal amplitudes substantially. The study suggests that improvements to the diurnal cycle in current models require improvements to the parameterized deep convection schemes, including the coupling with the boundary layer, the characteristic timescale of convection adjustment, and the triggering process for nocturnal precipitation. C1 Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Lee, MI (reprint author), Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. EM milee@gmao.gsfc.nasa.gov RI Bell, Thomas/G-5425-2012; Kim, Kyu-Myong/G-5398-2014; OI Lee, Myong-In/0000-0001-8983-8624 NR 37 TC 18 Z9 19 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 30 PY 2007 VL 112 IS D16 AR D16111 DI 10.1029/2006JD008346 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 208QW UT WOS:000249335300003 ER PT J AU Cuzzi, J AF Cuzzi, Jeff TI Planets - The first movement SO NATURE LA English DT Editorial Material C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Cuzzi, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jcuzzi@arc.nasa.gov NR 13 TC 3 Z9 3 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 30 PY 2007 VL 448 IS 7157 BP 1003 EP 1003 DI 10.1038/4481003a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 205EU UT WOS:000249097600025 PM 17728747 ER PT J AU Watson, DM Bohac, CJ Hull, C Forrest, WJ Furlan, E Najita, J Calvet, N d'Alessio, P Hartmann, L Sargent, B Green, JD Kim, KH Houck, JR AF Watson, Dan M. Bohac, C. J. Hull, C. Forrest, William J. Furlan, E. Najita, J. Calvet, Nuria d'Alessio, Paola Hartmann, Lee Sargent, B. Green, Joel D. Kim, Kyoung Hee Houck, J. R. TI The development of a protoplanetary disk from its natal envelope SO NATURE LA English DT Article ID NGC-1333 IRAS-4; COLLISIONAL EXCITATION; PROTOSTELLAR DISKS; MOLECULAR CLOUD; EMISSION-LINES; WATER; DISTRIBUTIONS; MODELS; INFALL; GAS AB Class 0 protostars, the youngest type of young stellar objects, show many signs of rapid development from their initial, spheroidal configurations, and therefore are studied intensively for details of the formation of protoplanetary disks within protostellar envelopes. At millimetre wavelengths, kinematic signatures of collapse have been observed in several such protostars, through observations of molecular lines that probe their outer envelopes. It has been suggested that one or more components of the proto-multiple system NGC 1333-IRAS 4 (refs 1, 2) may display signs of an embedded region that is warmer and denser than the bulk of the envelope(3,4). Here we report observations that reveal details of the core on Solar System dimensions. We detect in NGC 1333-IRAS 4B a rich emission spectrum of H(2)O, at wavelengths 20-37 mu m, which indicates an origin in extremely dense, warm gas. We can model the emission as infall from a protostellar envelope onto the surface of a deeply embedded, dense disk, and therefore see the development of a protoplanetary disk. This is the only example of mid-infrared water emission from a sample of 30 class 0 objects, perhaps arising from a favourable orientation; alternatively, this may be an early and short-lived stage in the evolution of a protoplanetary disk. C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. Univ Calif Los Angeles, NASA, Astrobiol Inst, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. RP Watson, DM (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. EM dmw@pas.rochester.edu NR 23 TC 55 Z9 55 U1 1 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 30 PY 2007 VL 448 IS 7157 BP 1026 EP 1028 DI 10.1038/nature06087 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 205EU UT WOS:000249097600032 PM 17728752 ER PT J AU Kump, LR Barley, ME AF Kump, Lee R. Barley, Mark E. TI Increased subaerial volcanism and the rise of atmospheric oxygen 2.5 billion years ago SO NATURE LA English DT Article ID ARCHEAN ATMOSPHERE; MULTIPLE-SULFUR; BLACK SMOKERS; EVOLUTION; TIME; TECTONICS; SEDIMENTS; ISOTOPES; RATIOS; EARTH AB The hypothesis that the establishment of a permanently oxygenated atmosphere at the Archaean-Proterozoic transition (similar to 2.5 billion years ago) occurred when oxygen-producing cyanobacteria evolved(1) is contradicted by biomarker evidence for their presence in rocks 200 million years older(2). To sustain vanishingly low oxygen levels despite near-modern rates of oxygen production from similar to 2.7-2.5 billion years ago thus requires that oxygen sinks must have been much larger than they are now. Here we propose that the rise of atmospheric oxygen occurred because the predominant sink for oxygen in the Archaean era-enhanced submarine volcanism-was abruptly and permanently diminished during the Archaean-Proterozoic transition. Observations(3-5) are consistent with the corollary that subaerial volcanism only became widespread after a major tectonic episode of continental stabilization at the beginning of the Proterozoic. Submarine volcanoes are more reducing than subaerial volcanoes(6), so a shift from predominantly submarine to a mix of subaerial and submarine volcanism more similar to that observed today would have reduced the overall sink for oxygen and led to the rise of atmospheric oxygen. C1 Penn State Univ, NASA, Astrobiol Inst, University Pk, PA 16802 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Univ Western Australia, Sch Earth & Geog Sci, Crawley, WA 6009, Australia. RP Kump, LR (reprint author), Penn State Univ, NASA, Astrobiol Inst, 535 Deike Bldg, University Pk, PA 16802 USA. EM lkump@psu.edu RI Barley, Mark/A-3803-2008; Kump, Lee/H-8287-2012 NR 30 TC 134 Z9 137 U1 6 U2 66 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 30 PY 2007 VL 448 IS 7157 BP 1033 EP 1036 DI 10.1038/nature06058 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 205EU UT WOS:000249097600034 PM 17728754 ER PT J AU Wing, S Gjerloev, JW Johnson, JR Hoffman, RA AF Wing, Simon Gjerloev, Jesper W. Johnson, Jay R. Hoffman, R. A. TI Substorm plasma sheet ion pressure profiles SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETOSPHERIC SUBSTORMS; MODEL; ACCESS AB [1] The plasma sheet pressure, temperature, and density profiles inferred from DMSP observations are used to investigate substorm growth, expansion, early-recovery, and late-recovery phases. During the growth phase, the pressure peaks at the inner edge of the plasma sheet. The premidnight pressure peak is associated with the temperature peak, while the postmidnight peak is associated with the density enhancement. After the substorm onset, the pressure at the inner edge diminishes. Instead, the pressure peaks at premidnight from X =-10 to - 40 R-E, which can be associated with temperature enhancement. During the early and late recovery phases, the pressure peaks at postmidnight, which is associated with a cold, dense ion population, possibly resulting from ion outflow and the substorm current systems. In the near-Earth region, the entropy decreases after substorm onset, but the specific entropy appears to be roughly conserved. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. Princeton Plasma Phys Lab, Princeton, NJ 08543 USA. RP Wing, S (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM simon.wing@jhuapl.edu NR 21 TC 18 Z9 18 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 29 PY 2007 VL 34 IS 16 AR L16110 DI 10.1029/2007GL030453 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 208QO UT WOS:000249334500003 ER PT J AU Li, ZQ Xia, XG Cribb, M Mi, W Holben, B Wang, PC Chen, HB Tsay, SC Eck, TF Zhao, FS Dutton, EG Dickerson, RR AF Li, Zhanqing Xia, Xiangao Cribb, Maureen Mi, Wen Holben, Brent Wang, Pucai Chen, Hongbin Tsay, Si-Chee Eck, T. F. Zhao, Fengsheng Dutton, E. G. Dickerson, R. R. TI Aerosol optical properties and their radiative effects in northern China SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SATELLITE MEASUREMENTS; CLOUD ABSORPTION; CLIMATE RESPONSE; SURFACE; ATMOSPHERE; AERONET; TOP; SYSTEM; OCEANS; MODEL AB [1] As a fast developing country covering a large territory, China is experiencing rapid environmental changes. High concentrations of aerosols with diverse properties are emitted in the region, providing a unique opportunity for understanding the impact of environmental changes on climate. Until very recently, few observational studies were conducted in the source regions. The East Asian Study of Tropospheric Aerosols: An International Regional Experiment (EAST-AIRE) attempts to characterize the physical, optical and chemical properties of the aerosols and their effects on climate over China. This study presents some preliminary results using continuous high- quality measurements of aerosol, cloud and radiative quantities made at the first EAST-AIRE baseline station at Xianghe, about 70 km east of Beijing over a period of one year (September 2004 to September 2005). It was found that the region is often covered by a thick layer of haze (with a yearly mean aerosol optical depth equal to 0.82 at 500 nm and maximum greater than 4) due primarily to anthropogenic emissions. An abrupt "cleanup'' of the haze often took place in a matter of one day or less because of the passage of cold fronts. The mean single scattering albedo is approximately 0.9 but has strong day-to-day variations with maximum monthly averages occurring during the summer. Large aerosol loading and strong absorption lead to a very large aerosol radiative effect at the surface (the annual 24-hour mean values equals 24 Wm(-2)), but a much smaller aerosol radiative effect at the top of the atmosphere (one tenth of the surface value). The boundary atmosphere is thus heated dramatically during the daytime, which may affect atmospheric stability and cloud formation. In comparison, the cloud radiative effect at the surface is only moderately higher (-41 W m(-2)) than the aerosol radiative effect at the surface. C1 Univ Maryland, Dept Atmospher & Ocean Sci, Earth Syst Sci Intedisciplinary Ctr, College Pk, MD 20742 USA. Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China. Nanjing Univ Informat Sci & Technol, Nanjing, Peoples R China. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO 80305 USA. China Meteorol Adm, Natl Satellite Meterol Ctr, Beijing 100081, Peoples R China. RP Li, ZQ (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, Earth Syst Sci Intedisciplinary Ctr, College Pk, MD 20742 USA. RI ECK, THOMAS/D-7407-2012; Xia, Xiangao/G-5545-2011; Cribb, Maureen/K-1341-2013; Li, Zhanqing/F-4424-2010; Tsay, Si-Chee/J-1147-2014; Dickerson, Russell/F-2857-2010 OI Xia, Xiangao/0000-0002-4187-6311; Cribb, Maureen/0000-0002-9745-3676; Li, Zhanqing/0000-0001-6737-382X; Dickerson, Russell/0000-0003-0206-3083 NR 50 TC 66 Z9 84 U1 3 U2 37 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 29 PY 2007 VL 112 IS D22 AR D22S01 DI 10.1029/2006JD007382 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 208QY UT WOS:000249335500001 ER PT J AU Georgiou, CD Papapostolou, I Sun, H McKay, CP AF Georgiou, Christos D. Papapostolou, Ioannis Sun, Henry McKay, Christopher P. TI Superoxide radical assays and applications in Mars-like Atacama soils SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID X-RAY SPECTROMETER; MARTIAN SOIL; CHEMICAL-COMPOSITION; TITANIUM-DIOXIDE; LIMITATIONS; HYDROETHIDINE; FLUORESCENCE; REACTIVITY; PRODUCT; PROTON AB Soils on Mars are thought to accumulate superoxide radicals, as they are formed continually by UV radiation hits on basalt minerals. Yet, beyond electron paramagnetic resonance (EPR) spectroscopy, no other methods exist that detect and quantify superoxide radicals in soils. This study describes two such assays that are based on the reaction of superoxide radical with hydroethidine and oxidized cytochrome c. They are unique in being able to test unambiguously for the presence of superoxide in a soil matrix with a high level of accuracy. Applications with soils from the Atacama Desert showed that the sensitivity of the assays is equal to or greater than that of EPR spectroscopy. C1 Univ Patras, Dept Biol, Sect Genet Cell Biol & Dev, Patras 26100, Greece. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Desert Res Inst, Las Vegas, NV 89119 USA. RP Georgiou, CD (reprint author), Univ Patras, Dept Biol, Sect Genet Cell Biol & Dev, Patras 26100, Greece. EM c.georgiou@upatras.gr; henry.sun@dri.edu; cmckay@mail.arc.nasa.gov RI Georgiou, Christos/B-8354-2013 OI Georgiou, Christos/0000-0001-9707-0109 NR 22 TC 6 Z9 6 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD AUG 29 PY 2007 VL 112 IS G4 AR G04S13 DI 10.1029/2006JG000390 PG 6 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 208RH UT WOS:000249336400002 ER PT J AU Warren-Rhodes, K Weinstein, S Dohm, J Piatek, J Minkley, E Hock, A Cockell, CS Pane, D Ernst, LA Fisher, G Emani, S Waggoner, AS Cabrol, NA Wettergreen, DS Apostolopoulos, D Coppin, P Grin, E Diaz, C Moersch, J Oril, GG Smith, T Stubbs, K Thomas, G Wagner, M Wyatt, M AF Warren-Rhodes, K. Weinstein, S. Dohm, J. Piatek, J. Minkley, E. Hock, A. Cockell, C. S. Pane, D. Ernst, L. A. Fisher, G. Emani, S. Waggoner, A. S. Cabrol, N. A. Wettergreen, D. S. Apostolopoulos, D. Coppin, P. Grin, E. Diaz, Chong Moersch, J. Oril, G. G. Smith, T. Stubbs, K. Thomas, G. Wagner, M. Wyatt, M. TI Searching for microbial life remotely: Satellite-to-rover habitat mapping in the Atacama Desert, Chile SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID DNA EXTRACTION; FLUORESCENCE; SOIL; MICROORGANISMS; ARIDITY; SAMPLES AB The Atacama Desert, one of the most arid landscapes on Earth, serves as an analog for the dry conditions on Mars and as a test bed in the search for life on other planets. During the Life in the Atacama (LITA) 2004 field experiment, satellite imagery and ground-based rover data were used in concert with a `follow-the-water' exploration strategy to target regions of biological interest in two ( 1 coastal, 1 inland) desert study sites. Within these regions, environments were located, studied and mapped with spectroscopic and fluorescence imaging (FI) for habitats and microbial life. Habitats included aqueous sedimentary deposits ( e. g., evaporites), igneous materials ( e. g., basalt, ash deposits), rock outcrops, drainage channels and basins, and alluvial fans. Positive biological signatures ( chlorophyll, DNA, protein) were detected at 81% of the 21 locales surveyed with the FI during the long-range, autonomous traverses totaling 30 km. FI sensitivity in detecting microbial life in extreme deserts explains the high percentage of positives despite the low actual abundance of heterotrophic soil bacteria in coastal (< 1-10(4) CFU/g-soil) and interior (< 1-10(2) CFU/g-soil) desert soils. Remote habitat, microbial and climate observations agreed well with ground-truth, indicating a drier and less microbially rich interior compared to the relatively wetter and abundant biology of the coastal site where rover sensors detected the presence of fog and abundant surface lichens. LITA project results underscore the importance of an explicit focus by all engineering and science disciplines on microbially relevant scales ( mm to nm), and highlight the success of satellite-based and `follow-the-water' strategies for locating diverse habitats of biological promise and detecting the microbial hotspots within them. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Carnegie Mellon Univ, Mol Biosensor & Imaging Ctr, Pittsburgh, PA 15213 USA. Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. SETI Inst, Mountain View, CA 94043 USA. Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. Univ Catolica Norte, Antofagasta 0610, Chile. Univ Iowa, Dept Mech & Ind Engn, Iowa City, IA 52242 USA. RP Warren-Rhodes, K (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM kwarren-rhodes@mail.arc.nasa.gov RI Moersch, Jeffrey/F-7189-2010; Dohm, James/A-3831-2014 NR 43 TC 13 Z9 13 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD AUG 29 PY 2007 VL 112 IS G4 AR G04S05 DI 10.1029/2006JG000283 PG 17 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 208RH UT WOS:000249336400001 ER PT J AU Milliken, RE Mustard, JF Poulet, F Jouglet, D Bibring, JP Gondet, B Langevin, Y AF Milliken, Ralph E. Mustard, John F. Poulet, Francois Jouglet, Denis Bibring, Jean-Pierre Gondet, Brigitte Langevin, Yves TI Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL EMISSION SPECTROMETER; REFLECTANCE SPECTROSCOPY; MERIDIANI-PLANUM; WATER-CONTENT; INFRARED SPECTROMETER; SPECTRAL REFLECTANCE; GLOBAL DISTRIBUTION; PARTICLE-SIZE; NEAR-SURFACE; GROUND ICE AB Visible-near infrared reflectance spectra acquired by the Mars Express Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite (OMEGA) spectrometer are used to estimate the absolute water content within the uppermost fraction of the Martian regolith. This upper surface layer represents the boundary between the regolith and atmosphere; thus the amount of water stored in these two reservoirs and at this boundary is expected to vary spatially and temporally with changing equilibrium conditions. We have applied models derived from laboratory experiments relating the strength of the 3 mm hydration feature to absolute water content to OMEGA spectra acquired during the first similar to 1200 orbits of the Mars Express mission to estimate the H2O content of the Martian surface. Three methods were used to examine the strength of the 3 mm absorption: integrated band depth, apparent absorbance, and the effective single-particle absorption-thickness (ESPAT) parameter. Integrated band depth and apparent absorbance values are correlated to albedo when derived from reflectance spectra, implying that bright regions are more hydrated than dark regions. The ESPAT parameter, however, relies on single scattering albedo instead of reflectance and is capable of estimating absolute water content within +/- 1 wt.% H2O for a wide range of albedo values, compositions, and particle sizes. Applying this model to the OMEGA data reveals that bright and dark regions commonly have similar water contents in equatorial regions and the largest spatial variations in H2O occur as a function of latitude. Equatorial regions exhibit water contents in the range of similar to 2-5 wt.%, whereas latitudes higher than similar to 45 degrees N are characterized by a continuous increase in H2O with latitude from similar to 5-15 wt.%. Phyllosilicate and sulfate bearing terrains are more hydrated than average bright and dark regions and their locations are in widely separated areas of Noachian-aged material, suggesting chemical alteration by water-rock interaction may have been spatially extensive in the early history of Mars. C1 Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. IAS, F-91405 Orsay, France. RP Milliken, RE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ralph.milliken@jpl.nasa.gov NR 63 TC 59 Z9 59 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 29 PY 2007 VL 112 IS E8 AR E08S07 DI 10.1029/2006JE002853 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 208RV UT WOS:000249337800002 ER PT J AU Liu, D Tangborn, A Kuang, W AF Liu, Don Tangborn, Andrew Kuang, Weijia TI Observing system simulation experiments in geomagnetic data assimilation SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID ERROR STATISTICS; MHD SYSTEM; FIELD; MODEL; DYNAMO; MANTLE AB Observing System Simulation Experiments (OSSEs) have been carried out for a geomagnetic data assimilation system. The purpose of these experiments is to demonstrate how new algorithms for assimilating geomagnetic observations into a geodynamo model can be evaluated. A "nature'' run is carried out to establish a "true'' evolution of the Earth's core state, from which synthetic surface geomagnetic field observations are created. These observations are then assimilated into the geodynamo model using an optimal interpolation (OI) scheme. Model error is simulated by using a different Rayleigh number in the nature and model runs. Because the true core state evolution is known completely, the assimilation results can be evaluated in terms of any state variable and at any point in the computational domain. In this work we focus on the poloidal (observed) and toroidal (unobserved) components of the magnetic field throughout the outer core. Experiments are carried out using observations of different degrees and varying forecast error correlation length scales. We also investigate the impact of model error on the assimilation and on the accuracy of geomagnetic forecasts. Assimilation runs lasting about 90% of the magnetic free decay time show a positive impact on both components of magnetic field deep within the outer core. Forecasts of the surface magnetic field show much lower error growth, indicating that the initial condition used for the forecasts has been substantially improved through assimilation. C1 Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Liu, D (reprint author), Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. EM donliu@umbc.edu; tangborn@umbc.edu; weijia.kuang-1@nasa.gov RI Kuang, Weijia/K-5141-2012 OI Kuang, Weijia/0000-0001-7786-6425 NR 23 TC 17 Z9 17 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD AUG 29 PY 2007 VL 112 IS B8 AR B08103 DI 10.1029/2006JB004691 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 208SB UT WOS:000249338400002 ER PT J AU Yang, Y Gupta, MC Dudley, KL AF Yang, Yonglai Gupta, Mool C. Dudley, Kenneth L. TI Towards cost-efficient EMI shielding materials using carbon nanostructure-based nanocomposites SO NANOTECHNOLOGY LA English DT Article ID NANOTUBE-POLYMER COMPOSITES; MECHANICAL-PROPERTIES; ELECTRICAL-CONDUCTIVITY; FABRICATION; NANOFIBERS; MORPHOLOGY; RUBBER AB Using a combination of dispersing low-cost carbon nanofibers and a small quantity of carbon nanotubes within the polystyrene matrix, we have demonstrated the formation of a novel nanocomposite with superior microstructure and improved electromagnetic interference (EMI) shielding characteristic. This nanocomposite is very promising for use as an effective and practical EMI shielding material owing to its high shielding effectiveness, light weight, low cost, and easy processability. C1 Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. NASA Langley Res Ctr, Electmagnet & Sensors Res Branch, Hampton, VA 23681 USA. RP Gupta, MC (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. EM mgupta@virginia.edu NR 34 TC 64 Z9 65 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 J9 NANOTECHNOLOGY JI Nanotechnology PD AUG 29 PY 2007 VL 18 IS 34 AR 345701 DI 10.1088/0957-4484/18/34/345701 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 207VC UT WOS:000249278200024 ER PT J AU Montmessin, F Haberle, RM Forget, F Langevin, Y Clancy, RT Bibring, JP AF Montmessin, F. Haberle, R. M. Forget, F. Langevin, Y. Clancy, R. T. Bibring, J.-P. TI On the origin of perennial water ice at the south pole of Mars: A precession-controlled mechanism? SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GENERAL-CIRCULATION MODEL; ATMOSPHERIC CIRCULATION; SUMMER TEMPERATURES; MARTIAN ATMOSPHERE; LAYERED DEPOSITS; ANNUAL CYCLE; CLIMATE; CAP; SUBLIMATION; STABILITY AB The poles of Mars are known to have recorded recent (< 10(7) years) climatic changes. While the south polar region appears to have preserved its million-year-old environment from major resurfacing events, except for the small portion containing the CO(2) residual cap, the discovery of residual water ice units in areas adjacent to the cap provides compelling evidence for recent glaciological activity. The mapping and characterization of these H(2)O-rich terrains by Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite (OMEGA) on board Mars Express, which have supplemented earlier findings by Mars Odyssey and Mars Global Surveyor, have raised a number of questions related to their origin. We propose that these water ice deposits are the relics of Mars' orbit precession cycle and that they were laid down when perihelion was synchronized with northern summer, i.e., more than 10,000 years ago. We favor precession over other possible explanations because (1) as shown by our General Circulation Model (GCM) and previous studies, current climate is not conducive to the accumulation of water at the south pole due to an unfavorable volatile transport and insolation configuration, (2) the residual CO2 ice cap, which is known to cold trap water molecules on its surface and which probably controls the current extent of the water ice units, is geologically younger, (3) our GCM shows that 21,500 years ago, when perihelion occurred during northern spring, water ice at the north pole was no longer stable and accumulated instead near the south pole with rates as high as 1 mm yr(-1). This could have led to the formation of a meters-thick circumpolar water ice mantle. As perihelion slowly shifted back to the current value, southern summer insolation intensified and the water ice layer became unstable. The layer recessed poleward until the residual CO(2) ice cover eventually formed on top of it and protected water ice from further sublimation. In this polar accumulation process, water ice clouds play a critical role since they regulate the exchange of water between hemispheres. The so-called "Clancy effect,'' which sequesters water in the spring/summer hemisphere coinciding with aphelion due to cloud sedimentation, is demonstrated to be comparable in magnitude to the circulation bias forced by the north-to-south topographic dichotomy. However, we predict that the response of Mars' water cycle to the precession cycle should be asymmetric between hemispheres not only because of the topographic bias in circulation but also because of an asymmetry in the dust cycle. We predict that under a "reversed perihelion'' climate, dust activity during northern summer is less pronounced than during southern summer in the opposite perihelion configuration (i.e., today's regime). When averaged over a precession cycle, this reduced potential for dust lifting will force a significantly colder summer in the north and, by virtue of the Clancy effect, will curtail the ability of the northern hemisphere to transfer volatiles to the south. This process may have helped create the observed morphological differences in the layered deposits between the poles and could help explain the large disparity in their resurfacing ages. C1 NASA, Ames Res Ctr, Div Space Sci, Mountain View, CA 94035 USA. Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. Space Sci Inst, Bald Head Isl, NC 28461 USA. UPMC, IPSL, CNRS, Meteorol Dynam Lab, F-75005 Paris, France. UVSQ, IPSL, CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. RP Montmessin, F (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Mountain View, CA 94035 USA. EM franck.montmessin@aero.jussieu.fr NR 40 TC 22 Z9 22 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 28 PY 2007 VL 112 IS E8 AR E08S17 DI 10.1029/2007JE002902 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 208RT UT WOS:000249337600001 ER PT J AU Hung, WH Kumar, R Bushmaker, A Cronin, SB Bronikowski, MJ AF Hung, Wei Hsuan Kumar, Rajay Bushmaker, Adam Cronin, Stephen B. Bronikowski, Michael J. TI Rapid prototyping of three-dimensional microstructures from multiwalled carbon nanotubes SO APPLIED PHYSICS LETTERS LA English DT Article ID BUNDLE ARRAYS; GROWTH; MICROFABRICATION; EMISSION AB The authors report a method for creating three-dimensional carbon nanotube structures, whereby a focused laser beam is used to selectively burn local regions of a dense forest of multiwalled carbon nanotubes. Raman spectroscopy and scanning electron microscopy are used to quantify the threshold for laser burnout and depth of burnout. The minimum power density for burning carbon nanotubes in air is found to be 244 mu W/mu m(2). We create various three-dimensional patterns using this method, illustrating its potential use for the rapid prototyping of carbon nanotube microstructures. Undercut profiles, changes in nanotube density, and nanoparticle formation are observed after laser surface treatment and provide insight into the dynamic process of the burnout mechanism. C1 Univ So Calif, Dept Mat Sci, Los Angeles, CA 90089 USA. Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hung, WH (reprint author), Univ So Calif, Dept Mat Sci, Los Angeles, CA 90089 USA. EM scronin@usc.edu RI Kumar, Rajay/A-3831-2012 NR 25 TC 9 Z9 9 U1 1 U2 7 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 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD AUG 27 PY 2007 VL 91 IS 9 AR 093121 DI 10.1063/1.2778292 PG 3 WC Physics, Applied SC Physics GA 206AK UT WOS:000249156100113 ER PT J AU Picard, YN Caldwell, JD Twigg, ME Eddy, CR Mastro, MA Henry, RL Holm, RT AF Picard, Y. N. Caldwell, J. D. Twigg, M. E. Eddy, C. R., Jr. Mastro, M. A. Henry, R. L. Holm, R. T. TI Nondestructive analysis of threading dislocations in GaN by electron channeling contrast imaging SO APPLIED PHYSICS LETTERS LA English DT Article ID SURFACES; GROWTH; LAYERS AB Threading dislocations in metal-organic chemical-vapor grown GaN films were imaged nondestructively by the electron channeling contrast imaging (ECCI) technique. Comparisons between ECCI and cross-sectional transmission electron microscopy indicated that pure edge dislocations can be imaged in GaN by ECCI. Total threading dislocation densities were measured by ECCI for various GaN films on engineered 4H-SiC surfaces and ranged from 10(7) to 10(9) cm(-2). A comparison between the ultraviolet electroluminescent output measured at 380 nm and the total dislocation density as measured by ECCI revealed an inverse logarithmic dependence. (c) 2007 American Institute of Physics. C1 USN, Res Lab, Elect Sci & Technol Div, Washington, DC 20375 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. OAI, Cleveland, OH 44135 USA. Sest Inc, Cleveland, OH 44135 USA. RP Picard, YN (reprint author), USN, Res Lab, Elect Sci & Technol Div, Washington, DC 20375 USA. EM yoosuf.picard@nrl.navy.mil RI Caldwell, Joshua/B-3253-2008; OI Caldwell, Joshua/0000-0003-0374-2168; Picard, Yoosuf/0000-0002-2853-5213 NR 20 TC 25 Z9 25 U1 1 U2 9 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 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD AUG 27 PY 2007 VL 91 IS 9 AR 094106 DI 10.1063/1.2777151 PG 3 WC Physics, Applied SC Physics GA 206AK UT WOS:000249156100152 ER PT J AU Nelli, SM Murphy, JR Sprague, AL Boynton, WV Kerry, KE Janes, DM Metzger, AE AF Nelli, Steven M. Murphy, James R. Sprague, Ann L. Boynton, William V. Kerry, Kris E. Janes, Daniel M. Metzger, Albert E. TI Dissecting the polar dichotomy of the noncondensable gas enhancement on Mars using the NASA Ames Mars general circulation model SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GLOBAL DUST STORMS; TES NADIR DATA; MARTIAN ATMOSPHERE; NUMERICAL-SIMULATION; SURFACE; WINTER; WAVES; CO2; SPECTROSCOPY; LATITUDES AB The atmospheric processes underlying the observed spatial and temporal enhancement of noncondensing gases in Mars' atmosphere are investigated. The Gamma Ray Spectrometer (GRS) on board Mars Odyssey has obtained measurements indicating that the absolute and relative column abundance of noncondensing gases (primarily argon and nitrogen) maximizes at high latitudes in both hemispheres during winter as CO2 gas condenses and forms the seasonal polar ice cap. This condensing CO2 "leaves behind'' noncondensing gases whose local absolute and relative column abundances can increase at a rate controlled by mixing with less-enhanced air from lower latitudes. Understanding the processes responsible for the magnitude and seasonal variations of these enhancement values is an aid in understanding atmospheric transport processes. The NASA Ames Mars General Circulation Model is employed to help understand the atmospheric thermodynamical mechanisms that give rise to the observed temporal and magnitude variations in the polar enhancement values. The model produces a threefold noncondensable gas enhancement in the south polar region and an approximate 1.4-fold increase in noncondensables in the north polar region. These model results are temporally consistent with observed values, but the observed enhancement magnitudes exceed those modeled by up to a factor of two. The difference in strength and the season of formation between transient eddies in the southern and northern hemispheres may play a large role in determining the different character of the two polar enhancements. Model simulations also illuminate the effect that topography, orbital eccentricity, and atmospheric dust opacity have on producing the north versus south polar enhancement dichotomy. C1 Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Jet Propuls Lab, Pasadena, CA USA. CALTECH, Pasadena, CA 91125 USA. RP Nelli, SM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM snelli@umich.edu; murphy@nmsu.edu; sprague@lpl.arizona.edu; wboynton@lpl.arizona.edu; krisk@lpl.arizona.edu; buck@lpl.arizona.edu; albert.e.metzger@jpl.nasa.gov NR 46 TC 9 Z9 9 U1 1 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 AUG 25 PY 2007 VL 112 IS E8 AR E08S91 DI 10.1029/2006JE002849 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 204HD UT WOS:000249033600001 ER PT J AU Draper, SL Krause, D Lerch, B Locci, IE Doehnert, B Nigam, R Das, G Sickles, P Tabernig, B Reger, N Rissbacher, K AF Draper, S. L. Krause, D. Lerch, B. Locci, I. E. Doehnert, B. Nigam, R. Das, G. Sickles, P. Tabernig, B. Reger, N. Rissbacher, K. TI Development and evaluation of TiAl sheet structures for hypersonic applications SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE titanium aluminide; sheet; mechanical properties; fabrication AB A cooperative program between the National Aeronautics and Space Administration (NASA), the Austrian Space Agency (ASA), Pratt & Whitney, Engineering Evaluation and Design, and Plansee AG was undertaken to determine the feasibility of achieving significant weight reduction of hypersonic propulsion system structures through the utilization of TiAl. A trade study defined the weight reduction potential of TiAl technologies as 25-35% compared to the baseline Ni-base superalloy for a stiffener structure in an inlet, combustor, and nozzle section of a hypersonic scramjet engine. A scramjet engine inlet cowl flap was designed, along with a representative subelement, using design practices unique to TiAl. A subelement was fabricated and tested to assess fabricability and structural performance and validate the design system. The TiAl alloy selected was PLANSEE's third generation alloy Gamma Met PX,(1) a high temperature, high-strength gamma-TiAl alloy with high Nb content. Characterization of Gamma Met PX sheet, including tensile, creep, and fatigue testing was performed. Additionally, design-specific coupons were fabricated and tested in order to improve subelement test predictions. Based on the sheet characterization and results of the coupon tests, the subelement failure location and failure load were accurately predicted. (c) 2007 Elsevier B.V. All rights reserved. C1 NASA, Glenn Res Ctr, Cleveland, OH USA. Pratt & Whitney Aircraft, W Palm Beach, FL USA. Pratt & Whitney, E Hartford, CT USA. Engn Evaluat & Design, Florence, KY USA. Plansee AG, Reutte, Austria. RP Draper, SL (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM Susan.L.Draper@nasa.gov NR 8 TC 38 Z9 40 U1 0 U2 12 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 AUG 25 PY 2007 VL 464 IS 1-2 BP 330 EP 342 DI 10.1016/j.msea.2007.02.020 PG 13 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 179XF UT WOS:000247323100045 ER PT J AU Wilson, SA Howard, AD Moore, JM Grant, JA AF Wilson, Sharon A. Howard, Alan D. Moore, Jeffrey M. Grant, John A. TI Geomorphic and stratigraphic analysis of Crater Terby and layered deposits north of Hellas basin, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SOFT-SEDIMENT DEFORMATION; THERMAL EMISSION SPECTROMETER; GLOBAL SURVEYOR; ORBITER CAMERA; MARGARITIFER SINUS; MARTIAN HIGHLANDS; ICE-SHEET; ART.; DRAINAGE; SURFACE AB The geologic history of Crater Terby is developed through geomorphic and stratigraphic analyses within the regional context of the Hellas basin. Terby exhibits similar to 2-km-thick sequences of layers that consist of repetitive, subhorizontal and laterally continuous beds. The layers are predominantly fine-grained as indicated by their ease of aeolian erosion, although a few consolidated layers weather to form rubbly talus. The grain size or composition of the deposited materials fluctuated, producing layering, but the overall properties of the deposits are similar throughout the sequence and are comparable to layered deposits in other crater basins around Hellas. The original depositional geometry, physical and geological characteristics of the layers in Terby and the other basins lead us to favor a lacustrine origin, but a loess-like origin cannot be ruled out. The formation of the layers corresponds to a period when the circum-Hellas region may have been occupied by a lake(s) up to 3.6 km deep. Once the lake in Hellas decreased, the layers in Terby were incised by troughs and a moat-like depression. We attribute this erosion to scour beneath an ice cover due to a lack of integrated fluvial drainage or large aeolian deflation features. The presence of viscous flow features in a crater on Terby's northwestern rim and lobate features on Terby's crater floor are also indicative of ice. The lack of depositional features associated with the postulated glacial activity suggests there was a contemporaneous shallow ( ice-covered?) lake covering the floor of Terby that transported material into the greater Hellas basin. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr eart & Planetary Studies, Washington, DC 20560 USA. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Wilson, SA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr eart & Planetary Studies, Washington, DC 20560 USA. EM wilsons@si.edu; ah6p@virginia.edu; jeff.moore@nasa.gov; grantj@si.edu NR 89 TC 42 Z9 42 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 AUG 24 PY 2007 VL 112 IS E8 AR E08009 DI 10.1029/2006JE002830 PG 39 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 204HB UT WOS:000249033400001 ER PT J AU Li, J Li, J Weisz, E Zhou, DK AF Li, Jun Li, Jinlong Weisz, Elisabeth Zhou, Daniel K. TI Physical retrieval of surface emissivity spectrum from hyperspectral infrared radiances SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RADIATIVE-TRANSFER MODEL; ATMOSPHERIC PROFILES; TEMPERATURE; ALGORITHM; AIRS; VALIDATION; PRODUCTS; MOISTURE; SOUNDER AB Retrieval of temperature, moisture profiles and surface skin temperature from hyperspectral infrared (IR) radiances requires spectral information about the surface emissivity. Using constant or inaccurate surface emissivities typically results in large temperature and moisture profile errors, particularly over semi-arid or arid areas where the variation in emissivity is large both spectrally and spatially. A physically based algorithm has been developed to retrieve a hyperspectral IR emissivity spectrum simultaneously with the temperature and moisture profiles, as well as the surface skin temperature. To make the solution stable and efficient, the hyperspectral emissivity spectrum is represented by eigenvectors, derived from the laboratory measured hyperspectral emissivity database, in the retrieval process. Experience with Atmospheric InfraRed Sounder (AIRS) radiances shows that simultaneous retrieval of the emissivity spectrum and the sounding improves the surface skin temperature and temperature and moisture profiles, particularly in the near surface layer. C1 Univ Wisconsin, Inst Meteorol Satellite Studies, Madison, WI 53706 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Li, J (reprint author), Univ Wisconsin, Inst Meteorol Satellite Studies, 1225 W Dayton St,Room 201, Madison, WI 53706 USA. RI Li, Jun/H-3579-2015 OI Li, Jun/0000-0001-5504-9627 NR 23 TC 46 Z9 47 U1 3 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 23 PY 2007 VL 34 IS 16 AR L16812 DI 10.1029/2007GL030543 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 204EZ UT WOS:000249027800004 ER PT J AU Hickson, KM Keyser, LF Sander, SP AF Hickson, Kevin M. Keyser, Leon F. Sander, Stanley P. TI Temperature dependence of the HO2+ClO reaction. 2. Reaction kinetics using the discharge-flow resonance-fluorescence technique SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID RATE-CONSTANT; AB-INITIO; RELATIVE STABILITIES; VIBRATIONAL-SPECTRA; PRODUCT FORMATION; ANTARCTIC OZONE; HO2 RADICALS; FIRN AIR; 300 K; CLO AB The total rate coefficient, k(3), for the reaction HO2 + ClO -> products has been determined over the temperature range of 220-336 K at a total pressure of approximately 1.5 Torr of helium using the discharge-flow resonance-fluorescence technique. Pseudo-first-order conditions were used with both ClO and HO2 as excess reagents using four different combinations of precursor molecules. HO2 molecules were formed by using either the termolecular association of H atoms in an excess of O-2 or via the reaction of F atoms with an excess of H2O2. ClO molecules were formed by using the reaction of Cl atoms with an excess of O-3 or via the reaction of Cl atoms with Cl2O. Neither HO2 nor ClO were directly observed during the course of the experiments, but these species were converted to OH or Cl radicals, respectively, via reaction with NO prior to their observation. OH fluorescence was observed at 308 nm, whereas Cl fluorescence was observed at approximately 138 nm. Numerical simulations show that under the experimental conditions used secondary reactions did not interfere with the measurements; however, some HO2 was lost on conversion to OH for experiments in excess HO2. These results were corrected to compensate for the simulated loss. At 296 K, the rate coefficient was determined to be (6.4 +/- 1.6) x 10(-12) cm(3) molecule(-1) s(-1). The temperature dependence expressed in Arrhenius form is (1.75 +/- 0.52) x 10(-12) exp[(368 +/- 78)/T] cm(3) molecule(-1) s(-1). The Arrhenius expression is derived from a fit weighted by the reciprocal of the measurement errors of the individual data points. The uncertainties are cited at the level of two standard deviations and contain contributions from statistical errors from the data analysis in addition to estimates of the systematic experimental errors and possible errors from the applied model correction. C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Sander, SP (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ssander@jpl.nasa.gov RI Hickson, Kevin/A-2443-2012 OI Hickson, Kevin/0000-0001-8317-2606 NR 39 TC 10 Z9 10 U1 0 U2 4 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 AUG 23 PY 2007 VL 111 IS 33 BP 8126 EP 8138 DI 10.1021/jp0689464 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 200JD UT WOS:000248758800012 PM 17655283 ER PT J AU Feng, LA Harwood, RS Brugge, R O'Neill, A Froidevaux, L Schwartz, M Waters, JW AF Feng, Liang Harwood, R. S. Brugge, R. O'Neill, A. Froidevaux, L. Schwartz, M. Waters, J. W. TI Equatorial Kelvin waves as revealed by EOS Microwave Limb Sounder observations and European Centre for Medium-Range Weather Forecasts analyses: Evidence for slow Kelvin waves of zonal wave number 3 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LOWER STRATOSPHERE; AURA SATELLITE; ASSIMILATION; TEMPERATURE; OSCILLATION; SIGNATURES; PROFILES; SPECTRA; SYSTEM; MLS AB Temperature and ozone observations from the Microwave Limb Sounder (MLS) on the EOS Aura satellite are used to study equatorial wave activity in the autumn of 2005. In contrast to previous observations for the same season in other years, the temperature anomalies in the middle and lower tropical stratosphere are found to be characterized by a strong wave-like eastward progression with zonal wave number equal to 3. Extended empirical orthogonal function (EOF) analysis reveals that the wave 3 components detected in the temperature anomalies correspond to a slow Kelvin wave with a period of 8 days and a phase speed of 19 m/s. Fluctuations associated with this Kelvin wave mode are also apparent in ozone profiles. Moreover, as expected by linear theory, the ozone fluctuations observed in the lower stratosphere are in phase with the temperature perturbations, and peak around 20-30 hPa where the mean ozone mixing ratios have the steepest vertical gradient. A search for other Kelvin wave modes has also been made using both the MLS observations and the analyses from one experiment where MLS ozone profiles are assimilated into the European Centre for Medium-Range Weather Forecasts (ECMWF) data assimilation system via a 6-hourly 3D var scheme. Our results show that the characteristics of the wave activity detected in the ECMWF temperature and ozone analyses are in good agreement with MLS data. C1 Univ Edinburgh, Inst Atmospher & Environm Sci, Edinburgh, Midlothian, Scotland. Univ Reading, Data Assimilat Res Ctr, Reading, Berks, England. CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Feng, LA (reprint author), Univ Edinburgh, Inst Atmospher & Environm Sci, Edinburgh, Midlothian, Scotland. RI Schwartz, Michael/F-5172-2016 OI Schwartz, Michael/0000-0001-6169-5094 NR 31 TC 5 Z9 5 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 22 PY 2007 VL 112 IS D16 AR D16106 DI 10.1029/2006JD008329 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 204FN UT WOS:000249029200003 ER PT J AU Mi, W Li, ZQ Xia, XG Holben, B Levy, R Zhao, FS Chen, HB Cribb, M AF Mi, Wen Li, Zhanqing Xia, Xiangao Holben, Brent Levy, Robert Zhao, Fengsheng Chen, Hongbin Cribb, Maureen TI Evaluation of the moderate resolution Imaging spectroradiometer aerosol products at two aerosol robotic network stations in china SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CLIMATE; ALGORITHM; RETRIEVAL; LAND AB Moderate Resolution Imaging Spectroradiometer (MODIS) aerosol products have been used to address aerosol climatic issues in many parts of the world, but their quality has yet to be determined over China. This paper presents a thorough evaluation of aerosol optical depth (AOD) data retrieved from MODIS collections 4 (C004) and 5 (C005) at two AERONET sites in northern and southeastern China. Established under the aegis of the East Asian Study of Tropospheric Aerosols: An International Regional Experiment (EAST-AIRE) project, the two sites, Xianghe and Taihu, have distinct ecosystems and climate regimes, resulting in differences in retrieval performance. At the rural northeastern site (Xianghe), MODIS C004 retrievals generally overestimate AOD at 550 nm during clean days, with the largest errors occurring during winter. In the warm and humid regions of southeastern China (Taihu), MODIS C004 retrievals overestimate AOD throughout the year. The systematic error at Xianghe is primarily due to the fixed surface reflectance ratio, while as the error at Taihu is mainly caused by the choice of the single scattering albedo (SSA) for the fine model aerosols. Both problems are alleviated considerably in the C005. The comparisons between C005 retrievals and AERONET data show much higher correlation coefficient, lower offset and a slope closer to unity. Also, the variability of AOD retrieval among neighboring pixels is reduced by several factors. The strong overestimation problem at small AOD values was fixed by using dynamic reflectance ratios that vary with the vegetation index and scattering angle. However, significant uncertainties remain because of the use of highly simplified aerosol models. C1 Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. Nanjing Univ Informat Sci & Technol, Sch Environm Sci & Engn, Nanjing, Peoples R China. Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. China Meteorol Adm, Natl Satellite Meteorol Ctr, Beijing, Peoples R China. RP Li, ZQ (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM zli@atmos.umd.edu RI Xia, Xiangao/G-5545-2011; Cribb, Maureen/K-1341-2013; Levy, Robert/M-7764-2013; Li, Zhanqing/F-4424-2010 OI Xia, Xiangao/0000-0002-4187-6311; Cribb, Maureen/0000-0002-9745-3676; Levy, Robert/0000-0002-8933-5303; Li, Zhanqing/0000-0001-6737-382X NR 27 TC 33 Z9 34 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 AUG 22 PY 2007 VL 112 IS D22 AR D22S8 DI 10.1029/2007JD008474 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 204FS UT WOS:000249029700001 ER PT J AU Skelley, AM Aubrey, AD Willis, PA Amashukeli, X Ehrenfreund, P Bada, JL Grunthaner, FJ Mathies, RA AF Skelley, Alison M. Aubrey, Andrew D. Willis, Peter A. Amashukeli, Xenia Ehrenfreund, Pascale Bada, Jeffrey L. Grunthaner, Frank J. Mathies, Richard A. TI Organic amine biomarker detection in the Yungay region of the Atacama Desert with the Urey instrument SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID SOIL-WATER BALANCE; MERIDIANI-PLANUM; ACID RACEMIZATION; MARS; LIFE; PRESERVATION; EXPLORATION; SEARCH; CHILE; ROVER AB The Urey in situ organic compound analysis instrument, consisting of a subcritical water extractor ( SCWE) and a portable microchip capillary electrophoresis instrument called the Mars Organic Analyzer ( MOA), was field tested in the Atacama Desert, Chile, in June 2005. Soil samples from the most arid Yungay region were collected, biomarkers were extracted by the SCWE, and organic amine composition and amino acid chirality analysis was performed by the MOA. Samples collected from the top 1 cm of duracrust soil but shielded from the ambient environment by rocks were compared to the exposed duracrust. The shielded duracrust yielded amines and amino acids ranging from 50 to 100 ppb, while amino acid signals from the exposed duracrust were below blank levels. Samples from buried gypsum deposits located directly above a water flow channel contained amino acids ranging from 13 to 90 ppb. Chiral analysis revealed D/L ratios of 0.39 +/- 0.08 and 0.34 +/- 0.07 for alanine/serine and 0.78 +/- 0.06 for aspartic acid, indicating significant racemization of biologically produced amino acids. On the basis of the D/L ratios, we estimate sample ages ranging from 10(3) to 10(5) years. These results demonstrate the successful field testing of the Urey instrument, as well as the detection of biomarkers from past terrestrial life in one of the most arid and Mars-like regions on Earth. C1 Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. Leiden Univ, Leiden Inst Chem, Astrobiol Lab, NL-2300 RA Leiden, Netherlands. RP Skelley, AM (reprint author), Univ Calif Berkeley, Dept Chem, MS 1460, Berkeley, CA 94720 USA. EM rich@zinc.cchem.berkeley.edu NR 45 TC 16 Z9 16 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD AUG 22 PY 2007 VL 112 IS G4 AR G04S11 DI 10.1029/2006JG000329 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 204FX UT WOS:000249030300001 ER PT J AU Eyring, V Waugh, DW Bodeker, GE Cordero, E Akiyoshi, H Austin, J Beagley, SR Boville, BA Braesicke, P Bruhl, C Butchart, N Chipperfield, MP Dameris, M Deckert, R Deushi, M Frith, SM Garcia, RR Gettelman, A Giorgetta, MA Kinnison, DE Mancini, E Manzini, E Marsh, DR Matthes, S Nagashima, T Newman, PA Nielsen, JE Pawson, S Pitari, G Plummer, DA Rozanov, E Schraner, M Scinocca, JF Semeniuk, K Shepherd, TG Shibata, K Steil, B Stolarski, RS Tian, W Yoshiki, M AF Eyring, V. Waugh, D. W. Bodeker, G. E. Cordero, E. Akiyoshi, H. Austin, J. Beagley, S. R. Boville, B. A. Braesicke, P. Bruehl, C. Butchart, N. Chipperfield, M. P. Dameris, M. Deckert, R. Deushi, M. Frith, S. M. Garcia, R. R. Gettelman, A. Giorgetta, M. A. Kinnison, D. E. Mancini, E. Manzini, E. Marsh, D. R. Matthes, S. Nagashima, T. Newman, P. A. Nielsen, J. E. Pawson, S. Pitari, G. Plummer, D. A. Rozanov, E. Schraner, M. Scinocca, J. F. Semeniuk, K. Shepherd, T. G. Shibata, K. Steil, B. Stolarski, R. S. Tian, W. Yoshiki, M. TI Multimodel projections of stratospheric ozone in the 21st century SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CHEMISTRY-CLIMATE MODEL; MIDDLE ATMOSPHERE MODEL; GASES NITROUS-OXIDE; WATER-VAPOR; INTERACTIVE CHEMISTRY; GREENHOUSE GASES; INTERANNUAL VARIABILITY; FUTURE CONCENTRATIONS; CIRCULATION MODEL; ART. AB Simulations from eleven coupled chemistry-climate models (CCMs) employing nearly identical forcings have been used to project the evolution of stratospheric ozone throughout the 21st century. The model-to-model agreement in projected temperature trends is good, and all CCMs predict continued, global mean cooling of the stratosphere over the next 5 decades, increasing from around 0.25 K/decade at 50 hPa to around 1 K/decade at 1 hPa under the Intergovernmental Panel on Climate Change ( IPCC) Special Report on Emissions Scenarios (SRES) A1B scenario. In general, the simulated ozone evolution is mainly determined by decreases in halogen concentrations and continued cooling of the global stratosphere due to increases in greenhouse gases (GHGs). Column ozone is projected to increase as stratospheric halogen concentrations return to 1980s levels. Because of ozone increases in the middle and upper stratosphere due to GHG-induced cooling, total ozone averaged over midlatitudes, outside the polar regions, and globally, is projected to increase to 1980 values between 2035 and 2050 and before lowerstratospheric halogen amounts decrease to 1980 values. In the polar regions the CCMs simulate small temperature trends in the first and second half of the 21st century in midwinter. Differences in stratospheric inorganic chlorine (Cl-y) among the CCMs are key to diagnosing the intermodel differences in simulated ozone recovery, in particular in the Antarctic. It is found that there are substantial quantitative differences in the simulated Cly, with the October mean Antarctic Cly peak value varying from less than 2 ppb to over 3.5 ppb in the CCMs, and the date at which the Cly returns to 1980 values varying from before 2030 to after 2050. There is a similar variation in the timing of recovery of Antarctic springtime column ozone back to 1980 values. As most models underestimate peak Cly near 2000, ozone recovery in the Antarctic could occur even later, between 2060 and 2070. In the Arctic the column ozone increase in spring does not follow halogen decreases as closely as in the Antarctic, reaching 1980 values before Arctic halogen amounts decrease to 1980 values and before the Antarctic. None of the CCMs predict future large decreases in the Arctic column ozone. By 2100, total column ozone is projected to be substantially above 1980 values in all regions except in the tropics. C1 Deutsches Zent Luft & Raunfahrt, Inst Atmospher Phys, Oberpfaffenhofen, Germany. Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. Natl Inst Water & Atmospher Res, Lauder, New Zealand. San Jose State Univ, Dept Meteorol, San Jose, CA 95192 USA. Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 2R7, Canada. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Univ Cambridge, Ctr Atmospher Sci, Cambridge, England. Max Planck Inst Chem, D-55128 Mainz, Germany. Met Off Climate Res Div, Exeter, Devon, England. Univ Leeds, Inst Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England. Meteorol Res Inst, Tsukuba, Ibaraki, Japan. Sci Syst & Applicat Inc, Lanham, MD USA. Max Planck Inst Meteorol, Hamburg, Germany. Univ Aquila, Dipartimento Fis, I-67100 Laquila, Italy. Ist Nazl Geofis & Vulcanol, Ctr Euro Mediterraneo Cambiamenti Climat, Bologna, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Environm Canada, Atomospher Environm Serv, Toronto, ON M3H 5T4, Canada. World Radiat Ctr, Inst Atmospher & Climate Sci ETHZ, Phys Meteorol Observ, Davos, Switzerland. ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. Univ Victoria, Canadian Ctr Climate Modelling & Anal, Meteorol Serv Canada, Victoria, BC, Canada. Univ Toronto, Dept Phys, Toronto, ON, Canada. RP Eyring, V (reprint author), Deutsches Zent Luft & Raunfahrt, Inst Atmospher Phys, Oberpfaffenhofen, Germany. EM veronika.eyring@dlr.de RI Rozanov, Eugene/A-9857-2012; Newman, Paul/D-6208-2012; Stolarski, Richard/B-8499-2013; Chipperfield, Martyn/H-6359-2013; Braesicke, Peter/D-8330-2016; Pawson, Steven/I-1865-2014; Waugh, Darryn/K-3688-2016; Marsh, Daniel/A-8406-2008; Manzini, Elisa/H-5760-2011; Pitari, Giovanni/O-7458-2016; Eyring, Veronika/O-9999-2016 OI Mancini, Eva/0000-0001-7071-0292; Rozanov, Eugene/0000-0003-0479-4488; Newman, Paul/0000-0003-1139-2508; Stolarski, Richard/0000-0001-8722-4012; Chipperfield, Martyn/0000-0002-6803-4149; Braesicke, Peter/0000-0003-1423-0619; Pawson, Steven/0000-0003-0200-717X; Waugh, Darryn/0000-0001-7692-2798; Marsh, Daniel/0000-0001-6699-494X; Pitari, Giovanni/0000-0001-7051-9578; Eyring, Veronika/0000-0002-6887-4885 NR 79 TC 200 Z9 209 U1 4 U2 42 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 21 PY 2007 VL 112 IS D16 AR D16303 DI 10.1029/2006JD008332 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 204FL UT WOS:000249029000005 ER PT J AU Fairlie, TD Avery, MA Pierce, RB Al-Saadi, J Dibb, J Sachse, G AF Fairlie, T. Duncan Avery, Melody A. Pierce, R. Bradley Al-Saadi, Jassim Dibb, Jack Sachse, Glen TI Impact of multiscale dynamical processes and mixing on the chemical composition of the upper troposphere and lower stratosphere during the Intercontinental Chemical Transport Experiment-North America SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ISENTROPIC-SIGMA MODEL; CHAOTIC ADVECTION; TROPOPAUSE FOLDS; OZONE BUDGET; JET-STREAM; ER-2 DATA; CHEMISTRY; EXCHANGE; ROSSBY; VORTEX AB We use high-frequency in situ observations made from the DC8 to examine fine-scale tracer structure and correlations observed in the upper troposphere and lower stratosphere during INTEX-NA. Two flights of the NASA DC-8 are compared and contrasted. Chemical data from the DC-8 flight on 18 July show evidence for interleaving and mixing of polluted and stratospheric air masses in the vicinity of the subtropical jet in the upper troposphere, while on 2 August the DC-8 flew through a polluted upper troposphere and a lowermost stratosphere that showed evidence of an intrusion of polluted air. We compare data from both flights with RAQMS 3-D global meteorological and chemical model fields to establish dynamical context and to diagnose processes regulating the degree of mixing on each day. We also use trajectory mapping of the model fields to show that filamentary structure due to upstream strain deformation contributes to tracer variability observed in the upper troposphere. An Eulerian measure of strain versus rotation in the large-scale flow is found useful in predicting filamentary structure in the vicinity of the jet. Higher-frequency ( 6 - 24 km) tracer variability is attributed to buoyancy wave oscillations in the vicinity of the jet, whose turbulent dissipation leads to efficient mixing across tracer gradients. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. Univ New Hampshire, Coll Engn & Phys Sci, Durham, NH 03824 USA. RP Fairlie, TD (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM t.d.fairlie@larc.nasa.gov RI Pierce, Robert Bradley/F-5609-2010 OI Pierce, Robert Bradley/0000-0002-2767-1643 NR 58 TC 9 Z9 9 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 21 PY 2007 VL 112 IS D16 AR D16S90 DI 10.1029/2006JD007923 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 204FL UT WOS:000249029000001 ER PT J AU Nedoluha, GE Alfred, J Benson, CM Hoppel, KW Wickert, J Koenig-Langlo, G AF Nedoluha, Gerald E. Alfred, Jerome Benson, Craig M. Hoppel, Karl W. Wickert, Jens Koenig-Langlo, Gert TI A comparison of radiosonde and GPS radio occultation measurements with meteorological temperature analyses in the Antarctic vortex, 1998-2004 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ART.; VALIDATION; PROFILES; OZONE; CHAMP AB We present comparisons between temperature measurements from sondes launched from South Pole Station and Neumayer Station with four meteorological analyses for the years 1998 - 2004. We also compare these meteorological analyses with inside-the-vortex GPS radio occultation measurements from the Challenging Minisatellite Payload ( CHAMP) instrument for 2001 - 2004. We use these comparisons to evaluate the interannual consistency of four meteorological analyses. We find that over the 1998 - 2004 period each of the four analyses showed at least one year-to-year jump in the average 1 June to 30 September bias of > 2.3 K when compared to the Neumayer and South Pole sondes at 30 hPa and 50 hPa. We find that while for the one nonoperational analysis ( the NCEP Reanalysis) the biases relative to sondes and GPS radio occultation measurements are often larger than for the operational analyses, the NCEP Reanalysis does show the best interannual consistency at 50 hPa. Having compared the meteorological analyses with measurements and with each other, we investigate whether the unusually high ozone at the top of the ozone hole (similar to 30 hPa) in 2003 can be understood in terms of unusually warm temperatures which would reduce the rate of chlorine activation and hence ozone destruction. We find that when bias corrections based on analysis-sonde comparisons are applied none of the meteorological analyses studied indicate that the winter of 2003 was warmer at 30 hPa than that of 1998 and 2000, years which did not show unusually high ozone at 30 hPa. C1 USN, Res Lab, Washington, DC 20375 USA. Computat Phys Inc, Springfield, VA USA. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. Goddard Earth Sci & Technol Ctr, Baltimore, MD USA. Geoforschungszentrum Potsdam, D-14473 Potsdam, Germany. Alfred Wegener Inst Polar & Marine Res, D-2850 Bremerhaven, Germany. RP Nedoluha, GE (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM nedoluha@nrl.navy.mil RI Wickert, Jens/A-7257-2013; Konig-Langlo, Gert/K-5048-2012 OI Konig-Langlo, Gert/0000-0002-6100-4107 NR 28 TC 3 Z9 3 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 21 PY 2007 VL 112 IS D16 AR D16304 DI 10.1029/2007Jd008928 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 204FL UT WOS:000249029000007 ER PT J AU Olsen, MA Schoeberl, MR Nielsen, JE AF Olsen, Mark A. Schoeberl, Mark R. Nielsen, J. Eric TI Response of stratospheric circulation and stratosphere-troposphere exchange to changing sea surface temperatures SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID DOUBLED CO2 CLIMATE; GENERAL-CIRCULATION; MIDDLE ATMOSPHERE; MODEL ASSESSMENT; TRANSPORT MODEL; MASS-EXCHANGE; ART.; TRENDS; OZONE; SIMULATION AB The Goddard Earth Observing System, version 4 general circulation model (GCM) is used to examine the influence of sea surface temperatures (SSTs) on stratospheric circulation and extratropical stratosphere-troposphere exchange (STE). The simulation uses observed SSTs from 1949 to 1998 at the lower boundary. The atmospheric greenhouse gas (GHG) burden is interannually constant to artificially decouple the radiative influence from the SST forcing. A stronger SST gradient from the tropics through the middle latitudes results in a greater meridional temperature gradient in the subtropical troposphere. The upper tropospheric zonal winds increase consistent with the thermal wind relationship, and vertically propagating waves are refracted more poleward into the stratosphere. As a consequence, the stratospheric residual circulation is strengthened. This is manifest as a net annual mass STE increase of 2.7% per decade in the Northern Hemisphere and 2.0% per decade in the Southern Hemisphere. Likewise, the characteristic residence time of air in the lowermost stratosphere decreases by about a month. The STE trends and upper tropospheric temperature gradients are not significantly different in a second simulation that specifies an increasing GHG burden. The second simulation also shows that the radiative cooling from an increased GHG burden is greater in magnitude than the SST-induced dynamical warming in the polar stratosphere. The results of this study imply that the modeled circulation of the stratosphere can be significantly affected by the SSTs. It follows that the fidelity of simulations of the 21st century atmosphere strongly depends on the SSTs, whether prescribed or interactive. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Olsen, MA (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, 5523 Res Pk Dr,Suite 320, Baltimore, MD 21228 USA. EM olsen@hyperion.gsfc.nasa.gov NR 29 TC 27 Z9 28 U1 0 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 AUG 21 PY 2007 VL 112 IS D16 AR D16104 DI 10.1029/2006JD008012 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 204FL UT WOS:000249029000002 ER PT J AU Safrankova, J Nemecek, Z Prech, L Samsonov, AA Koval, A Andreeova, K AF Safrankova, J. Nemecek, Z. Prech, L. Samsonov, A. A. Koval, A. Andreeova, K. TI Modification of interplanetary shocks near the bow shock and through the magnetosheath SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND SHOCK; EARTHS MAGNETOSPHERE; MAGNETIC CLOUD; MAGNETOPAUSE; WAVES; PROPAGATION AB [1] Fast forward interplanetary (IP) shocks have been identified as a source of the largest geomagnetic disturbances. These shocks can evolve in the solar wind, and they are modified both by interaction with the bow shock and during their propagation through the magnetosheath. Our contribution continues the study of the evolution of IP shocks in the magnetosheath. We compare profiles of the magnetic field and plasma parameters observed in the magnetosheath with profiles of the same parameters predicted by an MHD magnetosheath numerical model. The IP shock transmission into and its propagation through the magnetosheath cause inward and then outward motions of the bow shock, and these motions result in an "indentation'' of the bow shock surface. This indentation ( trough) flows along the bow shock together with the IP shock. Furthermore, we found that the interaction of the IP shock with the bow shock results in two discontinuities. These effects are consistent with the simulations of the MHD magnetosheath model. C1 Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic. St Petersburg State Univ, Dept Theoret Phys, Inst Phys, St Petersburg 198904, Russia. St Petersburg State Univ, Dept Theoret Phys, Inst Phys, St Petersburg 198904, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Safrankova, J (reprint author), Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic. EM jana.safrankova@mff.cuni.cz; zdenek.nemecek@mff.cuni.cz RI Samsonov, Andrey/I-7057-2012 OI Samsonov, Andrey/0000-0001-8243-1151 NR 26 TC 27 Z9 27 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 21 PY 2007 VL 112 IS A8 AR A08212 DI 10.1029/2007JA012503 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 204HO UT WOS:000249034800001 ER PT J AU McKernan, B Yaqoob, T Reynolds, CS AF McKernan, B. Yaqoob, T. Reynolds, C. S. TI A soft X-ray study of type I active galactic nuclei observed with Chandra high-energy transmission grating spectrometer SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques : spectroscopic; Galaxy : disc; galaxies : active; galaxies : Seyfert; X-rays : galaxies ID DUSTY WARM ABSORBER; XMM-NEWTON OBSERVATIONS; IONIZED-GAS; PHYSICAL CONDITIONS; NARROW-LINE; INTRINSIC ABSORPTION; SEYFERT-1 GALAXIES; SPACE-TELESCOPE; BLACK-HOLES; SPECTROSCOPY AB We present the results of a uniform analysis of the soft X-ray spectra of 15 type I active galactic nuclei (AGN) observed with the high-resolution X-ray gratings onboard Chandra. We found that 10 out of the 15 AGN exhibit signatures of an intrinsic ionized absorber. The absorbers are photoionized and outflowing, with velocities in the range similar to 10(1) - 10(3) km s(-1). The column density of the warm absorbing gas is similar to 10(23-23) cm(-2). Nine out of the 10 AGN exhibiting warm absorption are best fitted by multiple ionization components and three out of the 10 AGN require multiple kinematic components. The warm absorbing gas in our AGN sample has a wide range of ionization parameter, spanning roughly four orders of magnitude (xi similar to 10(0-4) erg cm s(-1)) in total, and often spanning three orders of magnitude in the same gas. Warm absorber components with ionization parameter xi < 10 generate an unresolved transition array due to Fe in seven out of the 10 AGN exhibiting warm absorption. These low ionization state absorbers may also carry away the largest mass outflows from the AGN. The mass outflow rate depends critically on the volume filling factor of the gas, which cannot yet be directly measured. However, upper limits on the mass outflow rates for filling factors of unity can be much greater than the expected accretion rate on to the central supermassive black hole and filling factors as small as 1 per cent can give outflow rates comparable to the accretion rate. There appears to be a gap in the outflow velocities in our sample between similar to 300 and 500 km s(-1), the origin of which is not clear. The outflow components with velocities below this gap tend to be associated with lower column densities than those with velocities above the gap. C1 CUNY, Borough Manhattan Community Coll, Dept Sci, New York, NY 10007 USA. Amer Museum Nat Hist, Dept Astrophys, Hayden Planetarium, Hayden Associate, New York, NY 10024 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP McKernan, B (reprint author), CUNY, Borough Manhattan Community Coll, Dept Sci, New York, NY 10007 USA. EM mckernan@astro.umd.edu NR 56 TC 107 Z9 107 U1 0 U2 2 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2007 VL 379 IS 4 BP 1359 EP 1372 DI 10.1111/j.1365-2966.2007.11993.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 209GP UT WOS:000249377300010 ER PT J AU Adams, JH ChriStl, MJ Howell, LW Kuznetsov, E AF Adams, J. H., Jr. ChriStl, M. J. Howell, L. W. Kuznetsov, E. TI The zero-degree detector system for fragmentation studies SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 11th Symposium on Rediation Measurements and Applications CY MAY 23-26, 2006 CL Univ Michigan, Ann Arbor, MI HO Univ Michigan DE ion fragments; cross-section; heavy-ion collision; galactic cosmic radiation; radiation transport model AB The measurement of nuclear fragmentation cross-sections requires the detection and identification of individual projectile fragments. If light and heavy fragments are recorded in the same detector, it may be impossible to distinguish the signal from the light fragment. To overcome this problem, we have developed the Zero-degree Detector System (ZDDS). The ZDDS enables the measurement of cross-sections for light fragment production by using pixelated detectors to separately measure the signals of each fragment. The system has been used to measure the fragmentation of beams as heavy as Fe at the NASA Space Radiation Laboratory at Brookhaven National Laboratory and the Heavy Ion Medical Accelerator in Chiba, Japan. Published by Elsevier B.V. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Alabama, Huntsville, AL 35899 USA. Moscow MV Lomonosov State Univ, Moscow 119992, Russia. RP Adams, JH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM james.h.adams@nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD AUG 21 PY 2007 VL 579 IS 1 BP 443 EP 446 DI 10.1016/j.nima.2007.04.094 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 208VX UT WOS:000249348400107 ER PT J AU Adams, JH Adcock, L Apple, J Christl, M Cleveand, W Cox, M Dietz, K Ferguson, C Fountain, W Ghita, B Kuznetsov, E Milton, M Myers, J O'Brien, S Seaquist, J Smith, EA Smith, G Warden, L Watts, J AF Adams, James H. Adcock, Leonard Apple, Jeffery Christl, Mark Cleveand, William Cox, Mark Dietz, Kurt Ferguson, Cynthia Fountain, Walt Ghita, Bogdan Kuznetsov, Evgeny Milton, Martha Myers, Jeremy O'Brien, Sue Seaquist, Jim Smith, Edward A. Smith, Guy Warden, Lance Watts, John TI Deep space test bed for radiation studies SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 11th Symposium on Rediation Measurements and Applications CY MAY 23-26, 2006 CL Univ Michigan, Ann Arbor, MI HO Univ Michigan DE galactic cosmic radiation; radiation shielding; radiation transport codes; long duration balloon flights AB The Deep Space Test-Bed (DSTB) Facility is designed to investigate the effects of galactic cosmic rays on crews and systems during missions to the Moon or Mars. To gain access to the interplanetary ionizing radiation environment the DSTB uses high-altitude polar balloon flights. The DSTB provides a platform for measurements to validate the radiation transport codes that are used by NASA to calculate the radiation environment within crewed space systems. It is also designed to support other exploration related investigations such as measuring the shielding effectiveness of candidate spacecraft and habitat materials, testing new radiation monitoring instrumentation, flight avionics and investigating the biological effects of deep space radiation. We describe the work completed thus far in the development of the DSTB and its current status. Published by Elsevier B.V. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Alabama, Huntsville, AL 35899 USA. Univ Space Res Assoc, Huntsville, AL 35806 USA. RP Adams, JH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM james.h.adams@nasa.gov NR 7 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD AUG 21 PY 2007 VL 579 IS 1 BP 522 EP 525 DI 10.1016/j.nima.2007.04.114 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 208VX UT WOS:000249348400127 ER PT J AU Zhao, K Zhang, A Lo, YH Farr, W AF Zhao, Kai Zhang, Arthur Lo, Yu-Hwa Farr, William TI InGaAs single photon avalanche detector with ultralow excess noise SO APPLIED PHYSICS LETTERS LA English DT Article ID PHOTODIODES AB An InGaAs single photon avalanche detector capable of sub-Geiger mode (Photomultiplier-tube-like) operation is reported. The device achieves a stable gain at around 10(6). The gain fluctuation is greatly suppressed through a self-quenching effect, thus an equivalent excess noise factor as low as 1.001 is achieved. In the photon counting experiment, the device is operated in the nongated mode under a dc bias. Because of its unique characteristics of self-quenching and self-recovery, no external quenching circuit is needed. The device shows a single photon response of around 30 ns and a self-recovery time of about 300 ns. (c) 2007 American Institute of Physics. C1 Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. Univ Calif San Diego, ECE Dept, La Jolla, CA 92093 USA. Jet Prop Lab, Pasadena, CA 91011 USA. RP Zhao, K (reprint author), Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. EM kzhao@physics.ucsd.edu NR 16 TC 26 Z9 26 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD AUG 20 PY 2007 VL 91 IS 8 AR 081107 DI 10.1063/1.2772231 PG 3 WC Physics, Applied SC Physics GA 203OV UT WOS:000248984800007 ER PT J AU Khan, SA Shafer, RA Serjeant, S Willner, SP Pearson, CP Benford, DJ Staguhn, JG Moseley, SH Sumner, TJ Ashby, MLN Borys, CK Chanial, P Clements, DL Dowell, CD Dwek, E Fazio, GG Kovacs, A Le Floc'h, E Silverberg, RF AF Khan, Sophia A. Shafer, Richard A. Serjeant, Stephen Willner, S. P. Pearson, Chris P. Benford, Dominic J. Staguhn, Johannes G. Moseley, S. Harvey Sumner, Timothy J. Ashby, Matthew L. N. Borys, Colin K. Chanial, Pierre Clements, David L. Dowell, C. Darren Dwek, Eli Fazio, Giovanni G. Kovacs, Attila Le Floc'h, Emeric Silverberg, Robert F. TI First constraints on source counts at 350 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : galaxies; galaxies : high-redshift; galaxies : starburst; submillimeter ID STAR-FORMATION HISTORY; HUBBLE-DEEP-FIELD; SUBMILLIMETER-SELECTED GALAXIES; SPITZER-SPACE-TELESCOPE; NUMBER COUNTS; HIGH-REDSHIFT; LOCKMAN HOLE; SHARC-II; EVOLUTION; SCUBA AB We have imaged a similar to 6 arcmin(2) region in the Bootes Deep Field using the 350 mu m-optimized second-generation Submillimeter High Angular Resolution Camera (SHARC II), achieving a peak 1 sigma sensitivity of similar to 5 mJy. We detect three sources above 3 sigma, and determine a spurious source detection rate of 1.09 in our maps. In the absence of 5 sigma detections, we rely on deep 24 mu m and 20 cm imaging to deduce which sources are most likely to be genuine, giving two real sources. From this we derive an integral source count of 0. 84(-0.61)(+1.39) sources arcmin(-2) at S > 13 mJy, which is consistent with 350 mu m source count models that have an IR-luminous galaxy population evolving with redshift. We use these constraints to consider the future for ground-based short-submillimeter surveys. C1 NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. European Space Agcy, ISO Data Ctr, Madrid 28080, Spain. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Khan, SA (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. RI Benford, Dominic/D-4760-2012; Moseley, Harvey/D-5069-2012; Dwek, Eli/C-3995-2012; Kovacs, Attila/C-1171-2010 OI Benford, Dominic/0000-0002-9884-4206; Kovacs, Attila/0000-0001-8991-9088 NR 51 TC 16 Z9 16 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2007 VL 665 IS 2 BP 973 EP 979 DI 10.1086/519239 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DK UT WOS:000248676200007 ER PT J AU Tavecchio, F Maraschi, L Ghisellini, G Kataoka, J Foschini, L Sambruna, RM Tagliaferri, G AF Tavecchio, F. Maraschi, L. Ghisellini, G. Kataoka, J. Foschini, L. Sambruna, R. M. Tagliaferri, G. TI Low-energy cutoffs and hard X-ray spectra in high-z radio-loud quasars: The Suzaku view of RBS 315 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : jets; quasars : individual (RBS 315); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; HIGH-REDSHIFT QUASARS; JET-DISK CONNECTION; WARM ABSORBER; BOARD SUZAKU; BLAZARS; DISTRIBUTIONS; LUMINOSITY; COMPTONIZATION AB We present the results from the Suzaku observation of the powerful radio-loud quasar RBS 315 (z = 2.69), for which a previous XMM-Newton observation showed an extremely flat X-ray continuum up to 10 keV ( photon index Gamma = 1.26) and indications of strong intrinsic absorption (N-H similar to 10(22) cm(-2), assuming neutral gas). The instrument for hard X-rays, HXD/PIN, allows us a detection of the source up to 50 keV. The broadband continuum (0.5-50 keV) can be well modeled with a power law with slope Gamma = 1.5 (definitively softer than the continuum measured by XMM-Newton) above 1 keV with strong deficit of soft photons. The low-energy cutoff can be well fitted, either with intrinsic absorption ( with column density N-H similar to 10(22) cm(-2) in the quasar rest frame) or with a break in the continuum, with an extremely hard (Gamma = 0.7) power law below 1 keV. We construct the spectral energy distribution of the source, using also optical-UV measurements obtained through a quasi-simultaneous observation with UVOT on board Swift observation. The shape of the SED is similar to that of other flat-spectrumradio quasars (FSRQs) with similar power, making this source an excellent candidate for the detection in gamma-rays by the Gamma-Ray Large Area Space Telescope ( GLAST). We model the SED with the synchrotron inverse Compton model usually applied to FSRQs, showing that the deficit of soft photons can be naturally interpreted as due to an intrinsic curvature of the spectrum near the low-energy end of the IC component, rather than to intrinsic absorption, although the latter possibility cannot be ruled out. We propose that in at least a fraction of the radio-loud QSOs at high redshift, the cutoff in the soft X-ray band can be explained in a similar way. Further studies are required to distinguish between the two alternatives. C1 Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. Osserv Astron Brera, INAF, I-20121 Milan, Italy. Tokio Inst Technol, Tokyo 1528551, Japan. IASF Bologna, INAF, I-40129 Bologna, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tavecchio, F (reprint author), Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy. RI Foschini, Luigi/H-3833-2012; XRAY, SUZAKU/A-1808-2009; OI Foschini, Luigi/0000-0001-8678-0324; Ghisellini, Gabriele/0000-0002-0037-1974; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 52 TC 42 Z9 42 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 AUG 20 PY 2007 VL 665 IS 2 BP 980 EP 989 DI 10.1086/519156 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DK UT WOS:000248676200008 ER PT J AU Sambruna, RM Reeves, JN Braito, V AF Sambruna, R. M. Reeves, J. N. Braito, V. TI The remarkable X-ray spectrum of the broad-line radio galaxy 3C 445 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON; ASCA OBSERVATIONS; SEYFERT-GALAXIES; SIMULTANEOUS RXTE; OPTICAL-SPECTRA; 3C 445; REFLECTION; EMISSION; ALPHA AB We present the results of the analysis of an archival 15 ks XMM-Newton observation of the nearby (z = 0.057) radio-loud source 3C 445, optically classified as a broad-line radio galaxy. While the RGS data are of insufficient quality to allow a meaningful analysis, the EPIC data show a remarkable X-ray spectrum. The 2-10 keV continuum is described by a heavily absorbed (N-H similar to 10(22)-10(23) cm(-2)) power law with photon index Gamma similar to 1.4 and strong ( R similar to 2) cold reflection. A narrow, unresolved FeK alpha emission line is detected, confirming previous findings, with EW similar to 120 eV. A soft excess is present below 2 keV over the extrapolation of the hard X-ray power law, which we model with a power law with the same photon index as the hard power law, absorbed by a column density N-H = 6 x 10(20) cm(-2) in excess to Galactic. A host of emission lines are present below 2 keV, confirming previous indications from ASCA, due to H- and He- like O, Mg, and Si. We attribute the origin of the lines to a photoionized gas, with properties very similar to radio-quiet obscured AGNs. Two different ionized media, or a single stratified medium, are required to fit the soft X-ray data satisfactorily. The similarity of the X-ray spectrum of 3C 445 to Seyferts underscores that the central engines of radio-loud and radio-quiet AGNs similarly host both cold and warm gas. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Sambruna, RM (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM rms@milkyway.gsfc.nasa.gov OI Braito, Valentina/0000-0002-2629-4989 NR 55 TC 26 Z9 26 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2007 VL 665 IS 2 BP 1030 EP 1037 DI 10.1086/519306 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DK UT WOS:000248676200012 ER PT J AU Grady, CA Schneider, G Hamaguchi, K Sitko, ML Carpenter, WJ Hines, D Collins, KA Williger, GM Woodgate, BE Henning, T Menard, F Wilner, D Petre, R Palunas, P Quirrenbach, A Nuth, JA Silverstone, MD Kim, JS AF Grady, C. A. Schneider, G. Hamaguchi, K. Sitko, M. L. Carpenter, W. J. Hines, D. Collins, K. A. Williger, G. M. Woodgate, B. E. Henning, Th. Menard, F. Wilner, D. Petre, R. Palunas, P. Quirrenbach, A. Nuth, J. A., III Silverstone, M. D. Kim, J. S. TI The disk and environment of a young Vega analog: HD 169142 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : visual; planetary systems : protoplanetary disks; stars : individual (2MASS 18242929-2946559, HD 22128, HD 36112, HD 142666, HD 169142, HD 220750); stars : low-mass, brown dwarfs; stars : pre-main-sequence ID HERBIG-AE/BE STARS; X-RAY-EMISSION; 2-DIMENSIONAL RADIATIVE-TRANSFER; HIGH-RESOLUTION SPECTROSCOPY; SPITZER-SPACE-TELESCOPE; RAPIDLY ROTATING STAR; MAIN-SEQUENCE STARS; T-TAURI STARS; AE STAR; PROTOSTELLAR ENVELOPES AB We trace the disk of HD169142 (A8 Ve) from 0.57" to 1.4" (approximate to 80-200 AU projected distance) in 1.1 mu m scattered light with HST NICMOS coronagraphy. The azimuthally symmetric disk has a peak azimuthally medianed surface brightness (SB) of approximate to 5 mJy arcsec(-2) at 0.57" from the star, and drops alpha r(-3). This radial SB profile is consistent with the presence of spatially resolved PAH emission and a Meeus group I IR SED only if the inner disk is either substantially flatter than the outer disk or partially devoid of material. Analysis of new HST ACS FUV imagery in tandem with archival IUE data indicates. M-acc <= 10(-9) M circle dot yr(-1). We estimate the age of HD 169142 to be 6(-3)(+6) Myr by identifying 2MASS 18242929-2946559, located 9.3" to the southwest, as a 130 mas separation weak-line T Tauri binary that is comoving with HD 169142 at the 4 sigma confidence level. We find no evidence for any additional stellar companion in either the ACS or Chandra ACIS-S data at r <= 1". HD 169142 has previously been interpreted as a slowly rotating, chemically peculiar star. However, by combining the disk inclination and v sin i from the literature, we find that the star has upsilon(equatorial) approximate to 240 km s(-1), making it a rapid rotator, similar to Altair or Vega. The UV data for HD 169142 are consistent with gravity darkening, while the X-ray luminosity and spectrum resembles early F stars at the age of the beta Pictoris moving group, rather than mid-A stars. In this context, spectral features previously interpreted as evidence for chemical peculiarity are more likely to reflect the presence of a strong photospheric latitudinal temperature gradient. With such a gradient, HD 169142 should closely resemble Vega at the epoch of central disk clearing. C1 Eureka Sci, Oakland, CA 96002 USA. NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. Space Sci Inst, Boulder, CO 80301 USA. Univ Cincinnati, Cincinnati, OH 45221 USA. Univ Louisville, Dept Phys, Louisville, KY 40292 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. CNRS, UJF UMR 5571, Lab Astrophys, Grenoble, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Heidelberg, Landessternwarte Konigstuhl, Zent Astron, D-69117 Heidelberg, Germany. NASA, Goddard Space Flight Ctr, Cosmochem Branch, Greenbelt, MD 20771 USA. RP Grady, CA (reprint author), Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA. RI Woodgate, Bruce/D-2970-2012; Nuth, Joseph/E-7085-2012 NR 79 TC 43 Z9 43 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2007 VL 665 IS 2 BP 1391 EP 1406 DI 10.1086/519757 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DK UT WOS:000248676200045 ER PT J AU Bolton, AS Burles, S Treu, T Koopmans, LVE Moustakas, LA AF Bolton, Adam S. Burles, Scott Treu, Tommaso Koopmans, Leon V. E. Moustakas, Leonidas A. TI A more fundamental plane SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular; cD; gravitational lensing ID EARLY-TYPE GALAXIES; DIGITAL SKY SURVEY; LENS ACS SURVEY; ELLIPTIC GALAXIES; GRAVITATIONAL LENS; FIELD GALAXIES; INTERMEDIATE-REDSHIFT; STELLAR POPULATIONS; SCALING RELATIONS; STAR-FORMATION AB We combine strong-lensing masses with SDSS stellar velocity dispersions and HST ACS effective (half-light) radii for 36 lens galaxies from the Sloan Lens ACS (SLACS) Survey to study the mass dependence of mass-dynamical structure in early-type galaxies. We find that over a 180-390 km s(-1) range in velocity dispersion, structure is independent of lensing mass to within 5%. This result suggests a systematic variation in the total (i.e., luminous plus dark matter) mass-to-light ratio as the origin of the "tilt" of the fundamental plane ( FP) scaling relationship between galaxy size, velocity dispersion, and surface brightness. We construct the FP of the lens sample, which we find to be consistent with the FP of the parent SDSS early-type galaxy population. We also present the first observational correlation between the mass-to-light ratio and residuals about the FP. Finally, we reformulate the FP in terms of surface mass density rather than surface brightness. By removing the complexities of stellar-population effects, this mass-plane formulation will facilitate comparison to numerical simulations and possible use as a cosmological distance indicator. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93101 USA. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bolton, AS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abolton@cfa.harvard.edu; burles@mit.edu; tt@physics.ucsb.edu; koopmans@astro.rug.nl; leonidas@jpl.nasa.gov NR 37 TC 53 Z9 53 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2007 VL 665 IS 2 BP L105 EP L108 DI 10.1086/521357 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DM UT WOS:000248676400006 ER PT J AU Bux, SK Blair, RG Gogna, P Kaner, RB Fleurial, JP AF Bux, Sabah K. Blair, Richard G. Gogna, Pawan Kaner, RIchard B. Fleurial, Jean-Pierre TI INOR 729-Synthesis and high temperature thermoelectric properties of some bulk nanostructured III-V semiconductors SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Bux, Sabah K.; Kaner, RIchard B.] Univ Calif Los Angeles, Dept Chem & Biochem, Los Angeles, CA 90095 USA. [Blair, Richard G.] Univ Cent Florida, Dept Chem, Orlando, FL 32816 USA. [Gogna, Pawan; Fleurial, Jean-Pierre] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM sabahkb@chem.ucla.edu; kaner@chem.ucla.edu; jean-pierre.fleurial@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 19 PY 2007 VL 234 MA 729-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V12IW UT WOS:000207593909039 ER PT J AU Cable, ML Kirby, JP Gray, HB Ponce, A AF Cable, Morgan L. Kirby, James P. Gray, Harry B. Ponce, Adrian TI INOR 663-Bacterial spore detection: Ionic radii effects on the stability of lanthanide ternary complexes SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Cable, Morgan L.; Gray, Harry B.] CALTECH, Beckman Inst, Pasadena, CA 91125 USA. [Kirby, James P.; Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Adrian.Ponce@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 19 PY 2007 VL 234 MA 663-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V12IW UT WOS:000207593909468 ER PT J AU Cozmuta, I Stolc, V AF Cozmuta, Ioana Stolc, Viktor TI COMP 145-Design of a protein ring sequencer via SMD simulations of RNA translocation SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Cozmuta, Ioana] NASA, Ames Res Ctr, Eloret Corp, Space Technol Div, Moffett Field, CA 94035 USA. EM icozmuta@mail.arc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 19 PY 2007 VL 234 MA 145-COMP PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V12IW UT WOS:000207593906156 ER PT J AU Cozmuta, I AF Cozmuta, Ioana TI COMP 342-Molecular mechanisms of gas surface interactions in hypersonic flow SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Cozmuta, Ioana] Eloret Corp, Space Technol Div, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM icozmuta@mail.arc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 19 PY 2007 VL 234 MA 342-COMP PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V12IW UT WOS:000207593906150 ER PT J AU Huang, XC Lee, TJ AF Huang, Xinchuan Lee, Timothy J. TI COMP 169-Highly accurate ab initio quartic force fields of C3H+and HO2+ SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Huang, Xinchuan; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM xhuang@mail.arc.nasa.gov; tjlee@mail.arc.nasa.gov RI HUANG, XINCHUAN/A-3266-2013 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 19 PY 2007 VL 234 MA 169-COMP PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V12IW UT WOS:000207593906140 ER PT J AU Shevade, AV Ryan, A Homer, M Blanco, M Goddard, WA AF Shevade, Abhijit V. Ryan, Amy Homer, Margie Blanco, Mario Goddard, William A. TI COMP 109-Quantum mechanical rapid screening of chemical sensing materials SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Shevade, Abhijit V.; Ryan, Amy; Homer, Margie] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Blanco, Mario; Goddard, William A.] CALTECH, Pasadena, CA 91125 USA. EM Abhijit.Shevade@jpl.nasa.gov; Margaret.A.Ryan@jpl.nasa.gov; mhomer@jpl.nasa.gov; mario@wag.caltech.edu; wag@wag.caltech.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 19 PY 2007 VL 234 MA 109-COMP PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V12IW UT WOS:000207593906407 ER PT J AU Son, KA Yang, BH Gallegos, M Liao, AN Prokopuk, N Moon, JS Yang, JW Khan, MA AF Son, Kyung-ah Yang, Baohua Gallegos, Manuel Liao, Anna Prokopuk, Nicholas Moon, Jeong S. Yang, Jinwei Khan, M. Asif TI COLL 75-Novel GaN-based chemical sensors for long-range chemical threat detection SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Son, Kyung-ah; Yang, Baohua; Gallegos, Manuel; Liao, Anna] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yang, Jinwei; Khan, M. Asif] Univ S Carolina, Columbia, SC 29208 USA. [Prokopuk, Nicholas] USN, Air Warfare Ctr, China Lake, CA 93555 USA. [Moon, Jeong S.] HRL Labs LLC, Malibu, CA 90265 USA. EM kson@jpl.nasa.gov; Baohua.Yang@jpl.nasa.gov; manuel.gallegos@jpl.nasa.gov; aliao@jpl.nasa.gov; nicholas.prokopuk@navy.mil; jmoon@hrl.com; yangj@engr.sc.edu; asif@engr.sc.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 19 PY 2007 VL 234 MA 75-COLL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V12IW UT WOS:000207593902261 ER PT J AU Xu, JC Hunter, GW Evans, LJ Vander Wal, RL Berger, GM Artale, M Lampard, P Androjna, D AF Xu, Jennifer C. Hunter, Gary W. Evans, Laura J. Vander Wal, Randy L. Berger, Gordon M. Artale, Mike Lampard, Peter Androjna, Drago TI INOR 489-The application of nanocrystalline and nanostructured metal oxides for chemical sensor development SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Xu, Jennifer C.; Hunter, Gary W.; Evans, Laura J.] NASA Glenn Res Ctr, Sensors & Elect Branch, Cleveland, OH 44135 USA. [Vander Wal, Randy L.; Berger, Gordon M.] NASA Glenn, USRA, Nanotechnol Lab, Cleveland, OH 44135 USA. [Artale, Mike; Lampard, Peter; Androjna, Drago] Sierra Lobo Inc, Cleveland, OH 44135 USA. EM Jennifer.C.Xu@nasa.gov; randy@rvander.grc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 19 PY 2007 VL 234 MA 489-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V12IW UT WOS:000207593909221 ER PT J AU Waliser, D Seo, KW Schubert, S Njoku, E AF Waliser, D. Seo, K.-W. Schubert, S. Njoku, E. TI Global water cycle agreement in the climate models assessed in the IPCC AR4 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LAND-SURFACE; FRESH-WATER; PRECIPITATION; ATMOSPHERE; DATASET; PROJECT AB This study examines the fidelity of the global water cycle in the climate model simulations assessed in the IPCC Fourth Assessment Report. The results demonstrate good model agreement in quantities that have had a robust global observational basis and that are physically unambiguous. The worst agreement occurs for quantities that have both poor observational constraints and whose model representations can be physically ambiguous. In addition, components involving water vapor ( frozen water) typically exhibit the best ( worst) agreement, and fluxes typically exhibit better agreement than reservoirs. These results are discussed in relation to the importance of obtaining accurate model representation of the water cycle and its role in climate change. Recommendations are also given for facilitating the needed model improvements. C1 CALTECH, Jet Prop Lab, Water & Carbon Cycles Grp, Pasadena, CA 91109 USA. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Waliser, D (reprint author), CALTECH, Jet Prop Lab, Water & Carbon Cycles Grp, 4800 Oak Grove Dr,MS 183-501, Pasadena, CA 91109 USA. EM waliser@caltech.edu NR 28 TC 15 Z9 15 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 18 PY 2007 VL 34 IS 16 AR L16705 DI 10.1029/2007GL030675 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 202JC UT WOS:000248896800005 ER PT J AU Del Genio, AD Yao, MS Jonas, J AF Del Genio, Anthony D. Yao, Mao-Sung Jonas, Jeffrey TI Will moist convection be stronger in a warmer climate? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID REANALYSIS DATA; CLOUDS; MICROPHYSICS; SATELLITE; MODELS; RADAR; FIRES; TRMM AB The intensity of moist convection is an important diagnostic of climate change not currently predicted by most climate models. We show that a simple estimate of the vertical velocity of convective updrafts in a global climate model reproduces observed land- ocean differences in convective intensity. Changes in convective intensity in a doubled CO2 simulation are small because the tropical lapse rate tends to follow a moist adiabatic profile. However, updrafts strengthen by similar to 1 m s(-1) with warming in the lightning- producing regions of continental convective storms, primarily due to an upward shift in the freezing level. For the western United States, drying in the warmer climate reduces the frequency of lightning- producing storms that initiate forest fires, but the strongest storms occur 26% more often. For the central- eastern United States, stronger updrafts combined with weaker wind shear suggest little change in severe storm occurrence with warming, but the most severe storms occur more often. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Sigma Space Partners LLC, New York, NY USA. Columbia Univ, New York, NY USA. RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM adelgenio@giss.nasa.gov RI Del Genio, Anthony/D-4663-2012 OI Del Genio, Anthony/0000-0001-7450-1359 NR 30 TC 66 Z9 66 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 AUG 17 PY 2007 VL 34 IS 16 AR L16703 DI 10.1029/2007GL030525 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 202JB UT WOS:000248896700005 ER PT J AU Ivins, ER Dokka, RK Blom, RG AF Ivins, Erik R. Dokka, Roy K. Blom, Ronald G. TI Post-glacial sediment load and subsidence in coastal Louisiana SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GLACIAL-ISOSTATIC-ADJUSTMENT; MISSISSIPPI RIVER DELTA; LAURENTIDE ICE-SHEET; GULF-OF-MEXICO; NEW-ORLEANS; SEA; HOLOCENE; FLUCTUATIONS; AMERICA; BARRIER AB Sea level rise in the Gulf of Mexico has occurred at a rate of 1.8-2.2 mm/yr during the 20th century, or nearly the same as observed globally due to combined steric and water mass changes. Tide gauges in coastal Louisiana, however, record a substantially larger rate of rise and while a number of causal mechanisms may be responsible, their specific contribution is poorly understood. Using a realistic viscoelastic Earth model, detailed geologic parameters for south Louisiana and new GPS data, we demonstrate that Holocene sedimentary loading in the Gulf and Mississippi River delta is capable of contributing to 1-8 mm/yr of subsidence over areas of 30-0.75 x 10(3) km(2). C1 CALTECH, Jet Prop Lab, Earth Sci Sect, Pasadena, CA 91109 USA. Louisiana State Univ, Dept Civil & Environm Engn, Baton Rouge, LA 70803 USA. Louisiana State Univ, Ctr Geoinformat, Baton Rouge, LA 70803 USA. RP Ivins, ER (reprint author), CALTECH, Jet Prop Lab, Earth Sci Sect, Mail Stop 300-233,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM eri@fryxell.jpl.nasa.gov NR 30 TC 39 Z9 40 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 17 PY 2007 VL 34 IS 16 AR L16303 DI 10.1029/2007GL030003 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 202JB UT WOS:000248896700002 ER PT J AU Chai, F Jiang, MS Chao, Y Dugdale, RC Chavez, F Barber, RT AF Chai, F. Jiang, M.-S. Chao, Y. Dugdale, R. C. Chavez, F. Barber, R. T. TI Modeling responses of diatom productivity and biogenic silica export to iron enrichment in the equatorial Pacific Ocean SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID PHYSICAL-BIOLOGICAL MODEL; FERTILIZATION EXPERIMENT; PHYTOPLANKTON BLOOM; SOUTHERN-OCEAN; NUTRIENT; GROWTH; CYCLE; DISSOLUTION; LIMITATION; NITRATE AB Using a three-dimensional physical-biogeochemical model, we have investigated the modeled responses of diatom productivity and biogenic silica export to iron enrichment in the equatorial Pacific, and compared the model simulation with in situ (IronEx II) iron fertilization results. In the eastern equatorial Pacific, an area of 540,000 km(2) was enhanced with iron by changing the photosynthetic efficiency and silicate and nitrogen uptake kinetics of phytoplankton in the model for a period of 20 days. The vertically integrated Chl a and primary production increased by about threefold 5 days after the start of the experiment, similar to that observed in the IronEx II experiment. Diatoms contribute to the initial increase of the total phytoplankton biomass, but decrease sharply after 10 days because of mesozooplankton grazing. The modeled surface nutrients (silicate and nitrate) and TCO2 anomaly fields, obtained from the difference between the "iron addition'' and "ambient'' (without iron) concentrations, also agreed well with the IronEx II observations. The enriched patch is tracked with an inert tracer similar to the SF6 used in the IronEx II. The modeled depth-time distribution of sinking biogenic silica (BSi) indicates that it would take more than 30 days after iron injection to detect any significant BSi export out of the euphotic zone. Sensitivity studies were performed to establish the importance of fertilized patch size, duration of fertilization, and the role of mesozooplankton grazing. A larger size of the iron patch tends to produce a broader extent and longer-lasting phytoplankton blooms. Longer duration prolongs phytoplankton growth, but higher zooplankton grazing pressure prevents significant phytoplankton biomass accumulation. With the same treatment of iron fertilization in the model, lowering mesozooplankton grazing rate generates much stronger diatom bloom, but it is terminated by Si(OH)(4) limitation after the initial rapid increase. Increasing mesozooplankton grazing rate, the diatom increase due to iron addition stays at minimum level, but small phytoplankton tend to increase. The numerical model experiments demonstrate the value of ecosystem modeling for evaluating the detailed interaction between biogeochemical cycle and iron fertilization in the equatorial Pacific. C1 Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. Univ Massachusetts, Environm Earth & Ocean Sci Dept, Boston, MA 02125 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. Duke Univ, Nicholas Sch Environm & Earth Sci, Marine Lab, Beaufort, NC 28516 USA. RP Chai, F (reprint author), Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. NR 59 TC 26 Z9 26 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD AUG 17 PY 2007 VL 21 IS 3 AR GB3S90 DI 10.1029/2006GB002804 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 202JE UT WOS:000248897000001 ER PT J AU Zaitchik, BF Evans, JP Smith, RB AF Zaitchik, Benjamin F. Evans, Jason P. Smith, Ronald B. TI Regional impact of an elevated heat source: The Zagros Plateau of Iran SO JOURNAL OF CLIMATE LA English DT Article ID BOUNDARY-LAYER; MESOSCALE MODEL; SOIL HYDROLOGY; VALIDATION; MONSOONS; WATER; CIRCULATIONS; REANALYSIS; CLIMATE; SYSTEM AB The authors propose that a heat- driven circulation from the Zagros Plateau has a significant impact on the climate of the Middle East Plain ( MEP), especially summertime winds, air temperature, and aridity. This proposal is examined in numerical experiments with a regional climate model. Simulations in which the Zagros Plateau was assigned a highly reflective, " snowlike" albedo neutralized the heat- driven circulation and produced an extra summertime warming of 1 degrees-2 degrees C in the MEP, measured relative to a control simulation and to the records of the NCEP - NCAR reanalysis project. This effect was largest in midsummer, when heating on the plateau was greatest. Additionally, simulations with high albedo on the Zagros showed reduced subsidence and enhanced precipitation in the MEP. These sensitivities are interesting because the Zagros Plateau lies downwind of the MEP. Analysis of model results indicates that the sensitivity of the upwind subsidence region to Zagros albedo can be understood as a linear atmospheric response to plateau heating, communicated upwind by a steady heat- driven circulation that influences the thermodynamic balance of the atmosphere. This regional phenomenon adds to the large- scale subsidence patterns established by the Hadley circulation and the Asian monsoon. Observed patterns of vertical motion in the Middle East, then, are a combined product of Zagros- induced subsidence and hemispheric- scale circulations. C1 Yale Univ, Dept Geol & Geophys, New Haven, CT USA. RP Zaitchik, BF (reprint author), Goddard Space Flight Ctr, Hydrol Sci Branch, Code 6143, Greenbelt, MD 20771 USA. EM bzaitchik@hsb.gsfc.nasa.gov RI Evans, Jason/F-3716-2011; Zaitchik, Benjamin/B-9461-2013 OI Evans, Jason/0000-0003-1776-3429; NR 35 TC 28 Z9 28 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD AUG 17 PY 2007 VL 20 IS 16 BP 4133 EP 4146 DI 10.1175/JCLI4248.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 201PS UT WOS:000248845700004 ER PT J AU Kar, J McElroy, CT Drummond, JR Zou, J Nichitiu, F Walker, KA Randall, CE Nowlan, CR Dufour, DG Boone, CD Bernath, PF Trepte, CR Thomason, LW McLinden, C AF Kar, Jayanta McElroy, C. Thomas Drummond, James R. Zou, Jason Nichitiu, Florian Walker, Kaley A. Randall, Cora E. Nowlan, Caroline R. Dufour, Denis G. Boone, Chris D. Bernath, Peter F. Trepte, Charles R. Thomason, Larry W. McLinden, Chris TI Initial comparison of ozone and NO2 profiles from ACE-MAESTRO with balloon and satellite data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID VALIDATION; SPECTROMETER; INSTRUMENT; IRRADIANCE; AEROSOL AB [1] Atmospheric retrievals of ozone and NO2 by the Measurements of Aerosol Extinction in the Stratosphere and Troposphere Retrieved by Occultation (MAESTRO) instrument which is part of the Atmospheric Chemistry Experiment ( ACE) satellite aboard SCISAT are compared statistically with coincident measurements by ozonesondes, the Fourier Transform Spectrometer (ACE-FTS) also aboard SCISAT, the SAGE III and the POAM III instruments. The ozone mixing ratio profiles from MAESTRO and ozonesondes agree within about 5-10% from 16-30 km in the northern middle and high latitudes. Further, ACE-FTS and MAESTRO ozone profiles agree within similar to 5- 15% from 16-50 km. MAESTRO ozone profiles show a systematic bias which is opposite for sunrise (SR) and sunset ( SS) events and was also seen in comparisons with SAGE III and POAM III ozone. MAESTRO SS ozone profiles mostly agree within 5-10% from 16-40 km with either SAGE III or POAM III SR or SS retrievals, but show a significant high bias from 40-55 km, reaching a maximum of similar to 20-30%. MAESTRO SR ozone profiles show a low bias of similar to 5- 15% from 20-50 km, as compared to SAGE III and POAM III SR or SS measurements. The NO2 profiles agree within about 10-15% between ACE-FTS and MAESTRO from 15-40 km for the SR and 22-35 km for the SS measurements. Further, MAESTRO NO2 profiles agree with SAGE III NO2 mostly within 10% from 25-40 km. MAESTRO NO2 profiles agree with POAM III SR profiles within 5-10% from 25-42 km. However, compared to POAM III SS profiles, MAESTRO NO2 profiles show a low bias between 20 and 25 km (similar to 30-50%), a high MAESTRO bias between 25 and 32 km (10-30%), and again a low bias above 33 km that increases with altitude to 50-60%. C1 Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Environm Canada, Meteorol Serv Canada, Downsview, ON M3H 5T4, Canada. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Kar, J (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM jkar@atmosp.physics.utoronto.ca RI McLinden, Chris/A-7710-2010; Bernath, Peter/B-6567-2012; Drummond, James/O-7467-2014; Randall, Cora/L-8760-2014 OI McLinden, Chris/0000-0001-5054-1380; Bernath, Peter/0000-0002-1255-396X; Nowlan, Caroline/0000-0002-8718-9752; Randall, Cora/0000-0002-4313-4397 NR 25 TC 13 Z9 14 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 17 PY 2007 VL 112 IS D16 AR D16301 DI 10.1029/2006JD008242 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 202JM UT WOS:000248897800001 ER PT J AU Durkin, GA Dowling, JP AF Durkin, Gabriel A. Dowling, Jonathan P. TI Local and global distinguishability in quantum interferometry SO PHYSICAL REVIEW LETTERS LA English DT Article ID PHASE MEASUREMENT; STATES; LIMIT; SU(2) AB A statistical distinguishability based on relative entropy characterizes the fitness of quantum states for phase estimation. This criterion is employed in the context of a Mach-Zehnder interferometer and used to interpolate between two regimes of local and global phase distinguishability. The scaling of distinguishability in these regimes with photon number is explored for various quantum states. It emerges that local distinguishability is dependent on a discrepancy between quantum and classical rotational energy. Our analysis demonstrates that the Heisenberg limit is the true upper limit for local phase sensitivity. Only the "NOON" states share this bound, but other states exhibit a better trade-off when comparing local and global phase regimes. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Louisiana State Univ, Hearne Inst Theoret Phys, Baton Rouge, LA 70803 USA. RP Durkin, GA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI DOWLING, JONATHAN/L-2749-2013 NR 31 TC 55 Z9 55 U1 1 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 17 PY 2007 VL 99 IS 7 AR 070801 DI 10.1103/PhysRevLett.99.070801 PG 4 WC Physics, Multidisciplinary SC Physics GA 201XW UT WOS:000248866900007 PM 17930881 ER PT J AU Paddack, SJ Rubincam, DP AF Paddack, Stephen J. Rubincam, David P. TI Explorer XII: Spinning faster than expected - Response SO SCIENCE LA English DT Letter C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Paddack, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Rubincam, David/D-2918-2012 NR 8 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD AUG 17 PY 2007 VL 317 IS 5840 BP 898 EP 899 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 200RJ UT WOS:000248780200018 ER PT J AU Zhang, LQ Li, HR Hu, XB Jalbout, AF AF Zhang, Liqun Li, Haoran Hu, Xingbang Jalbout, Abraham F. TI Theoretical study of the influence of ribose on the proton transfer phenomenon of nucleic acid bases SO CHEMICAL PHYSICS LA English DT Article DE ribose; uridine; DFT; proton transfer; influence ID DENSITY-FUNCTIONAL CALCULATIONS; GROUND-STATE PROPERTIES; POST-HARTREE-FOCK; AB-INITIO CALCULATIONS; ELECTRON-ATTACHMENT; URACIL-WATER; VIBRATIONAL PROPERTIES; AQUEOUS-SOLUTION; EXCESS ELECTRON; GUANINE AB The first comprehensive theoretical study of ribose's effects on the behavior of proton transfer of nucleic acid base is presented. The specific hydrogen bonding of the ribose hydroxyls plays a very important role in the stabilization of the structure of ribonucleoside. Nine stable uridine conformations have been reported. The intermolecular proton transfer of the isolated, monohydrated uridine complexes in three different regions were extensively explored on the basis of density functional theory at the B3LYP/6-31+G* level. With the introduction of the ribose, not only the structural parameters of the nucleic acid bases changed, but also the energy barriers of the proton transfer process changed. Furthermore, changes of the electron distributions of the molecular orbital of the nucleic acid bases were also analyzed by NBO analysis. Consideration of the ribose's influence represents a much more real situation in the RNA. (c) 2007 Elsevier B.V. All rights reserved. C1 Zhejiang Univ, Dept Chem, Hangzhou 310027, Peoples R China. Univ Nacl Autonoma Mexico, Inst Chem, Mexico City 04510, DF, Mexico. Univ Arizona, Dept Chem, NASA, Astrobiol Inst, Tucson, AZ 85721 USA. RP Li, HR (reprint author), Zhejiang Univ, Dept Chem, Hangzhou 310027, Peoples R China. EM lihr@zju.edu.cn; ajalbout@email.arizona.edu NR 45 TC 4 Z9 4 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD AUG 16 PY 2007 VL 337 IS 1-3 BP 110 EP 118 DI 10.1016/j.chemphys.2007.06.046 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 212YG UT WOS:000249632400012 ER PT J AU Stajner, I Benson, C Liu, HC Pawson, S Brubaker, N Chang, LP Riishojgaard, LP Todling, R AF Stajner, Ivanka Benson, Craig Liu, Hui-Chun Pawson, Steven Brubaker, Nicole Chang, Lang-Ping Riishojgaard, Lars Peter Todling, Ricardo TI Ice polar stratospheric clouds detected from assimilation of Atmospheric Infrared Sounder data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OZONE DEPLETION; AIRS; WINTER; WAVES AB A novel technique is presented for the detection and mapping of ice polar stratospheric clouds ( PSCs), using brightness temperatures from the Atmospheric Infrared Sounder ( AIRS) "moisture'' channel near 6.79 mu m. It is based on observed-minus-forecast residuals ( O-Fs) computed when using AIRS radiances in the Goddard Earth Observing System version 5 ( GEOS-5) data assimilation system. Brightness temperatures are computed from six-hour GEOS-5 forecasts using a radiation transfer module under clear-sky conditions, meaning they will be too high when ice PSCs are present. We study whether the O-Fs contain quantitative information about PSCs by comparison with sparse data from the Polar Ozone and Aerosol Measurement ( POAM) III solar occultation instrument. AIRS O-Fs lower than -2 K generally coincide with PSCs observed by POAM III. Synoptic maps of AIRS O-Fs lower than -2 K are constructed as a proxy for ice PSCs. These are used to investigate spatio-temporal variations of Antarctic PSCs in the year 2004. C1 Sci Applicat Int Corp, Beltsville, MD USA. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Stajner, I (reprint author), Sci Applicat Int Corp, Beltsville, MD USA. RI Stajner, Ivanka/B-5228-2009; Pawson, Steven/I-1865-2014 OI Stajner, Ivanka/0000-0001-6103-3939; Pawson, Steven/0000-0003-0200-717X NR 25 TC 7 Z9 7 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 16 PY 2007 VL 34 IS 16 AR L16802 DI 10.1029/2007GL029415 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 202IZ UT WOS:000248896500001 ER PT J AU Koenig, LS Steig, EJ Winebrenner, DP Shuman, CA AF Koenig, Lora S. Steig, Eric J. Winebrenner, Dale P. Shuman, Christopher A. TI A link between microwave extinction length, firn thermal diffusivity, and accumulation rate in West Antarctica SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID BRIGHTNESS TEMPERATURES; VARIABILITY; SURFACE; SSM/I; RECORDS; TRENDS AB The relationship between time series of physical surface temperature and microwave brightness temperature of polar firn depends both on the physical properties of the firn and the surface temperature history. In perennially dry firn this relationship is well characterized by a timescale, referred to as the extinction-diffusion time, which is the ratio of the microwave extinction length squared to the firn thermal diffusivity. The extinction-diffusion time is calculated over Antarctica from 1982 to 1999 by comparing thermal infrared observations of physical surface temperature from the advanced very high resolution radiometer ( AVHRR) with passive microwave brightness temperatures measured by the scanning multichannel microwave radiometer ( SMMR) and Special Senor Microwave Imager ( SSM/I). Independent estimates of accumulation rate are derived both from ice cores and from spatially extensive ground and airborne radar echo sounding lines. The extinction-diffusion time is found to vary linearly with accumulation rate from approximately 10 to 50 cm/yr ice equivalent over a large area in West Antarctica. Although this simple relationship does not appear to hold at very low or very high accumulation rates, these results suggest that the extinction-diffusion time holds promise as a viable proxy for accumulation rate variability on polar ice sheets. C1 Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. Univ Washington, Appl Phys Lab, Seattle, WA USA. NASA Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD USA. NASA Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD USA. RP Koenig, LS (reprint author), Univ Washington, Dept Earth & Space Sci, 70 Johnson Hall,Campus Box 351310, Seattle, WA 98195 USA. EM lorak@u.washington.edu; steig@u.washington.edu; dpw@apl.washington.edu; christopher.a.shuman@nasa.gov RI Steig, Eric/G-9088-2015 OI Steig, Eric/0000-0002-8191-5549 NR 26 TC 5 Z9 6 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD AUG 16 PY 2007 VL 112 IS F3 AR F03018 DI 10.1029/2006JF000716 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 202JZ UT WOS:000248899100002 ER PT J AU Hemant, K Thebault, E Mandea, M Ravat, D Maus, S AF Hemant, Kumar Thebault, Erwan Mandea, Mioara Ravat, Dhananjay Maus, Stefan TI Magnetic anomaly map of the world: merging satellite, airborne, marine and ground-based magnetic data sets SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE world digital magnetic anomaly map; LEEDS-WDMAM candidate model; aeromagnetic and marine compilation ID CHAMP; FIELD; NORTHERN; SURFACE; OCEAN AB We report here a simple but practical method to combine systematically the magnetic surveys of disparate specifications from marine, ground, aeromagnetic and satellite platforms that aims to be helpful in the framework of the world digital magnetic anomaly map project. Because the satellite coverage and data quality is more uniform than near-surface surveys, it is adopted as the base map for wavelengths larger than 400 kin and up to spherical harmonic degree inclusive of 16 (similar to 2500 km). After checking that satellite models and large aeromagnetic wavelengths are not consistent, we filter out wavelengths longer than 400 km in aeromagnetic compilations. Existing regional grids and, when available, individual surveys, are merged to give a more uniform spatial variation of the magnetic anomalies. The effects of merging the grids are examined by plotting profiles and difference maps of the overlapping regions. A preliminary global map is obtained after combining the magnetic anomaly map with the downward continued CHAMP satellite derived magnetic anomaly map. Forthcoming availability of new datasets, as well as improvements in the procedure, will help to produce increasingly reliable maps. (c) 2007 Elsevier B.V All rights reserved. C1 Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. GeoForsch Zentrum, Potsdam, Germany. Inst Phys Globe, Jussieu, France. So Illinois Univ Dale, Carbondale, IL USA. NOAA, Natl Geophys Data Ctr, Boulder, CO 80303 USA. RP Hemant, K (reprint author), Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. EM hemant@earth.leeds.ac.uk RI MANDEA, Mioara/E-4892-2012; Thebault, Erwan/A-5670-2011; OI Maus, Stefan/0000-0002-9604-3878; Ravat, Dhananjay/0000-0003-1962-4422 NR 33 TC 28 Z9 37 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD AUG 15 PY 2007 VL 260 IS 1-2 BP 56 EP 71 DI 10.1016/j.epsl.2007.05.040 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 202DX UT WOS:000248883300005 ER PT J AU Aumann, HH Gregorich, DT Broberg, SE Elliott, DA AF Aumann, Hartmut H. Gregorich, David T. Broberg, Steven E. Elliott, Denis A. TI Seasonal correlations of SST, water vapor, and convective activity in tropical oceans: A new hyperspectral data set for climate model testing SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB The analysis of the response of the Earth Climate System to the seasonal changes of solar forcing in the tropical oceans using four years of the Atmospheric Infrared Sounder (AIRS) and Advanced Microwave Sounding Unit (AMSU) data between 2002 and 2006 gives new insight into amplitude and phase relationships between surface and tropospheric temperatures, humidity, and convective activity. The intensity of the convective activity is measured by counting deep convective clouds. The peaks of convective activity, temperature in the mid-troposphere, and water vapor in the 0 - 30 N and 0 - 30 S tropical ocean zonal means occur about two months after solstice, all leading the peak of the sea surface temperature by several weeks. Phase is key to the evaluation of feedback. The evaluation of climate models in terms of zonal and annual means and annual mean deviations from zonal means can now be supplemented by evaluating the phase of key atmospheric and surface parameters relative to solstice. The ability of climate models to reproduce the statistical flavor of the observed amplitudes and relative phases for broad zonal means should lead to increased confidence in the realism of their water vapor and cloud feedback algorithms. AIRS and AMSU were launched into a 705 km altitude polar sun-synchronous orbit on the EOS Aqua spacecraft on May 4, 2002, and have been in routine data gathering mode since September 2002. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Aumann, HH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM aumann@jpl.nasa.gov NR 11 TC 7 Z9 7 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 AUG 15 PY 2007 VL 34 IS 15 AR L15813 DI 10.1029/2006GL029191 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 202IX UT WOS:000248896300001 ER PT J AU Gosling, JT Phan, TD Lin, RP Szabo, A AF Gosling, J. T. Phan, T. D. Lin, R. P. Szabo, A. TI Prevalence of magnetic reconnection at small field shear angles in the solar wind SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PLASMA AB A study of magnetic reconnection exhausts observed at high (3-s) temporal resolution by the plasma and magnetic field experiments on Wind during March 2006 reveals, unexpectedly, that reconnection in the solar wind occurs most frequently at field shear angles < 90 degrees. Owing largely to the relatively low reconnection rates associated with small field shear angles, the corresponding exhausts tend to be quite narrow (< 4 x 10(4) km) and typically are convected past the spacecraft by the solar wind flow in < 100 s. During March 2006 Wind encountered reconnection exhausts at an average rate of similar to 1.5 events/day, a factor of similar to 36 greater than has been inferred from previous observations, largely made at considerably lower (similar to 1-min) temporal resolution. C1 Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gosling, JT (reprint author), Univ Colorado, Atmospher & Space Phys Lab, 1234 Innovat Dr, Boulder, CO 80303 USA. EM jack.gosling@lasp.colorado.edu NR 15 TC 46 Z9 49 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 15 PY 2007 VL 34 IS 15 AR L15110 DI 10.1029/2007GL030706 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 202IX UT WOS:000248896300008 ER PT J AU Luttrell, K Sandwell, D Smith-Konter, B Bills, B Bock, Y AF Luttrell, Karen Sandwell, David Smith-Konter, Bridget Bills, Bruce Bock, Yehuda TI Modulation of the earthquake cycle at the southern San Andreas fault by lake loading SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID STRESS CHANGES; SLIP RATE; CALIFORNIA; RESERVOIR; SYSTEM; ACCUMULATION; DISPLACEMENT; DEFORMATION; SEISMICITY; NEVADA AB Changes in the level of ancient Lake Cahuilla over the last 1500 years in the Salton Trough alter the state of stress by bending the lithosphere in response to the applied lake load and by varying the pore pressure magnitude within the crust. The recurrence interval of the lake is similar to the recurrence interval of rupture on the southern San Andreas and San Jacinto faults, both of which are partially covered by the lake at its highstand. Furthermore, four of the last five ruptures on the southern San Andreas fault have occurred near a time of substantial lake level change. We investigate the effect of Coulomb stress perturbations on local faults due to changing level of Lake Cahuilla to determine a possible role for the lake in affecting the timing of fault rupture. Coulomb stress is calculated with a three-dimensional model of an elastic plate overlying a viscoelastic half-space. Plate thickness and half-space relaxation time are adjusted to match observed vertical deformation since the last lake highstand. The lake cycle causes positive and negative Coulomb stress perturbations of 0.2-0.6 MPa on the southern San Andreas within the lake and 0.1-0.2 MPa on the southern San Andreas outside the lake. These Coulomb stress perturbations are comparable to stress magnitudes known to have triggered events at other faults along the North America-Pacific plate boundary. C1 Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Luttrell, K (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM kluttrell@ucsd.edu RI Bills, Bruce/C-1156-2008; Smith-Konter, Bridget/D-2823-2011; Luttrell, Karen/D-6772-2015; OI Smith-Konter, Bridget/0000-0001-6004-1005; Sandwell, David/0000-0001-5657-8707 NR 42 TC 20 Z9 20 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD AUG 15 PY 2007 VL 112 IS B8 AR B08411 DI 10.1029/2006JB004752 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 202KJ UT WOS:000248900200001 ER PT J AU Ogilvie, KW Coplan, MA Roberts, DA Ipavich, F AF Ogilvie, K. W. Coplan, M. A. Roberts, D. A. Ipavich, F. TI Solar wind structure suggested by bimodal correlations of solar wind speed and density between the spacecraft SOHO and Wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; ALFVEN WAVES; PLASMA; FLUCTUATIONS; ORIGIN; PROPAGATION; SHOCKS AB [1] We calculate the cross-spacecraft maximum lagged-cross-correlation coefficients for 2-hour intervals of solar wind speed and density measurements made by the plasma instruments on the Solar and Heliospheric Observatory ( SOHO) and Wind spacecraft over the period from 1996, the minimum of solar cycle 23, through the end of 2005. During this period, SOHO was located at L1, about 200 RE upstream from the Earth, while Wind spent most of the time in the interplanetary medium at distances of more than 100 RE from the Earth. Yearly histograms of the maximum, time-lagged correlation coefficients for both the speed and density are bimodal in shape, suggesting the existence of two distinct solar wind regimes. The larger correlation coefficients we suggest are due to structured solar wind, including discontinuities and shocks, while the smaller are likely due to Alfvenic turbulence. While further work will be required to firmly establish the physical nature of the two populations, the results of the analysis are consistent with a solar wind that consists of turbulence from quiet regions of the Sun interspersed with highly filamentary structures largely convected from regions in the inner solar corona. The bimodal appearance of the distributions is less evident in the solar wind speed than in the density correlations, consistent with the observation that the filamentary structures are convected with nearly constant speed by the time they reach 1 AU. We also find that at solar minimum the fits for the density correlations have smaller high-correlation components than at solar maximum. We interpret this as due to the presence of more relatively uniform Alfvenic regions at solar minimum than at solar maximum. C1 NASA, Goddard Space Flight Ctr, Heliospher Sci Div, Greenbelt, MD 20771 USA. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RP Ogilvie, KW (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Sci Div, Greenbelt, MD 20771 USA. EM aaron.roberts@nasa.gov RI Roberts, Dana/D-4625-2012 NR 31 TC 4 Z9 4 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 15 PY 2007 VL 112 IS A8 AR A08104 DI 10.1029/2007JA012248 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 202KO UT WOS:000248900700002 ER PT J AU Roberts, DA Giacalone, J Jokipii, JR Goldstein, ML Zepp, TD AF Roberts, D. Aaron Giacalone, Joe Jokipii, J. R. Goldstein, Melvyn L. Zepp, Timothy D. TI Spectra of polar heliospheric fields and implications for field structure SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETIC-FIELD; CURRENT SHEET; SOLAR-WIND; ORIGIN; LATITUDE AB [1] The predictions of the " Fisk'' model for a peak at the equatorial solar rotation frequency in the spectrum of the latitudinal component of the heliospheric magnetic field were found to give values significantly larger than those observed. The observed values were statistically the same as observed in the ecliptic and were consistent with random fluctuations about the ( null) Parker field component. These conclusions are based on spectra of field and plasma quantities using Ulysses data from the first southern and northern polar passes. There was also no evidence for solar photospheric differential rotation in the latitudinal component. A related search for signatures of the differential rotation ( not directly part of the Fisk magnetic field model) yielded the strongest evidence for a photospheric influence on the radial component of the solar wind velocity and related " compressive'' quantities. C1 NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. Duke Univ, Dept Elect Engn, Durham, NC 27706 USA. RP Roberts, DA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RI Roberts, Dana/D-4625-2012; Goldstein, Melvyn/B-1724-2008 NR 12 TC 14 Z9 14 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 15 PY 2007 VL 112 IS A8 AR A08103 DI 10.1029/2007JA012247 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 202KO UT WOS:000248900700001 ER PT J AU Lee, J Bradshaw, RC Hyers, RW Rogers, JR Rathz, TJ Wall, JJ Choo, H Liaw, PK AF Lee, J. Bradshaw, R. C. Hyers, R. W. Rogers, J. R. Rathz, T. J. Wall, J. J. Choo, H. Liaw, P. K. TI Non-contact measurement of creep resistance of ultra-high-temperature materials SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article; Proceedings Paper CT Symposium on Processing and Mechanical Response of Engineering Materials held at the 2006 TMS Annual Meeting CY MAR 12-16, 2006 CL San Antonio, TX SP TMS DE creep; ultra-high-temperature; electrostatic levitation; finite element analysis; nuclear propulsion; hypersonic aircraft ID NICKEL-BASE SUPERALLOY; FINITE-ELEMENT MODEL; CONSTITUTIVE-EQUATIONS; ELEVATED-TEMPERATURES; MULTIAXIAL STRESS; REFRACTORY-METALS; FERRITIC STEEL; BEHAVIOR; ALLOY; COMPOSITES AB Continuing pressures for higher performance and efficiency in energy conversion and propulsion systems are driving ever more demanding needs for new materials which can survive high stresses at the elevated temperatures. In such severe environments, the characterization of creep properties becomes indispensable. Conventional techniques for the measurement of creep are limited to about 1700 degrees C. A new method which can be applied at temperatures higher than 2000 degrees C is strongly demanded. This paper presents a non-contact method for creep measurements of ultra-high-temperature materials at 2300 degrees C. Using the electrostatic levitation facility at NASA MSFC, a spherical sample was rotated quickly enough to cause creep deformation due to centripetal acceleration. The deformation of the sample was captured with a digital camera, and the images were analyzed to measure creep deformation. To validate experimental results, numerical and analytical analyses on creep deformation of a rotating sphere have been conducted. The experimental, numerical, and analytical results showed good agreement with one another. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Massachusetts, Amherst, MA 01003 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Alabama, Huntsville, AL 35899 USA. Univ Tennessee, Knoxville, TN 37996 USA. RP Hyers, RW (reprint author), Univ Massachusetts, Amherst, MA 01003 USA. EM hyers@ecs.umass.edu RI Hyers, Robert/G-3755-2010; Choo, Hahn/A-5494-2009 OI Choo, Hahn/0000-0002-8006-8907 NR 87 TC 8 Z9 8 U1 1 U2 12 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 EI 1873-4936 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD AUG 15 PY 2007 VL 463 IS 1-2 SI SI BP 185 EP 196 DI 10.1016/j.msea.2006.07.160 PG 12 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 182YA UT WOS:000247538700028 ER PT J AU Van Aalsburg, J Grant, LB Yakovlev, G Rundle, PB Rundle, JB Turcotte, DL Donnellan, A AF Van Aalsburg, Jordan Grant, Lisa B. Yakovlev, Gleb Rundle, Paul. B. Rundle, John B. Turcotte, Donald L. Donnellan, Andrea TI A feasibility study of data assimilation in numerical simulations of earthquake fault systems SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS LA English DT Article; Proceedings Paper CT AGU Western Pacific Geophysical Meeting CY JUL 24-28, 2006 CL Beijing, PEOPLES R CHINA SP AGU DE earthquakes; virtual california; numerical simulations; forecasting; data assimilation ID SAN-ANDREAS FAULT; PAST 500 YEARS; SOUTHERN-CALIFORNIA; SYNTHETIC SEISMICITY; MODEL; STATISTICS; RECURRENCE; RECORD; SITE AB Topologically realistic simulations of earthquake faults systems have been constructed to understand the physics of interacting earthquake fault systems. We focus on one of these models, a simulation called Virtual California, that represents a model for the strike-slip fault system in California. In weather forecasting, current and past observations are routinely extrapolated forward to forecast future weather. The question addressed in this paper is whether a similar application of numerical simulations can be used in earthquake forecasting. Present simulation models are discussed and their ability to successfully generate earthquake recurrence statistics is demonstrated. An important question relates to how paleoseismic data can be used to constrain simulations, and whether these constrained simulations provide improved forecasts of future earthquakes. Here, we show first results from a consideration of these issues using a method of "datascoring". The data are divided into "training intervals" and "testing intervals". In the training intervals. the time history of paleoseismic data are used to evaluate space-time windows of simulations. Earthquakes following high-scoring space-time windows in the simulations are then used as a basis for developing waiting time statistics and used to forecast data in the testing intervals. In our present method, we focus on the problem of determining the timing of future earthquakes having magnitude m > 7. Our preliminary conclusion is that the amount of paleoseismic data currently available does not as yet improve the waiting time statistics to a level significantly beyond a random (temporal) predictor. However, this conclusion is based on a set of studies that are not extensive, so further investigations may well reveal important new avenues. In particular, it may be that the true value of this approach lies in defining the probable spatial locations of future earthquakes, rather than their timing. Published by Elsevier B.V. C1 Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. Univ Calif Davis, Computat Sci & Engn Ctr, Davis, CA 95616 USA. Univ Calif Irvine, Program Publ Hlth, Irvine, CA 92697 USA. Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. Jet Propuls Lab, Pasadena, CA USA. RP Rundle, JB (reprint author), Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. EM jbrundle@ucdavis.edu RI Ludwig, Lisa Grant/G-6442-2012 OI Ludwig, Lisa Grant/0000-0001-6538-8067 NR 38 TC 6 Z9 6 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-9201 J9 PHYS EARTH PLANET IN JI Phys. Earth Planet. Inter. PD AUG 15 PY 2007 VL 163 IS 1-4 BP 149 EP 162 DI 10.1016/j.pepi.2007.04.020 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 210VH UT WOS:000249483200010 ER PT J AU Bane, JM Spitz, YH Letelier, RM Peterson, WT AF Bane, John M. Spitz, Yvette H. Letelier, Ricardo M. Peterson, William T. TI Jet stream intraseasonal oscillations drive dominant ecosystem variations in Oregon's summertime coastal upwelling system SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE coastal variability; wind-driven ocean upwelling; coastal marine; ecosystems; marine ecology ID NORTHERN CALIFORNIA CURRENT; SEA-LEVEL; WEST-COAST; WIND; VARIABILITY; SHELF AB Summertime wind stress along the coast of the northwestern United States typically exhibits intraseasonal oscillations MOO with periods from approximate to 15 to 40 days, as well as fluctuations on the 2-to 6-day "weather-band" and 1-day diurnal time scales. Coastal upwelling of cool, nutrient-rich water is driven by extended periods of equatorward alongshore winds, and we show that the approximate to 20-day ISOs in alongshore wind stress dominated the upwelling process during summer 2001 off Oregon. These wind stress ISOs resulted from north-south positional ISOs of the atmospheric jet stream (JS). Upper-ocean temperature, phytoplankton, and zoo-plankton varied principally on the approximate to 20-day time scale as well, and these correlated with the ISOs in alongshore wind stress and JS position, even though there also were weather-band stress fluctuations of comparable magnitude. Such wind stress ISOs are typical along Oregon in the summer upwelling season, occurring in 10 of 12 years examined, including 2001. We present a previously unreported direct connection from the atmospheric JS to oceanic primary and secondary production on the intraseasonal time scale and show the leading importance of ISOs in driving this coastal upwelling ecosystem during a typical summer. C1 Univ N Carolina, Dept Marine Sci, Chapel Hill, NC 27599 USA. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, Newport, OR 97365 USA. RP Bane, JM (reprint author), Univ N Carolina, Dept Marine Sci, Chapel Hill, NC 27599 USA. EM bane@unc.edu RI Letelier, Ricardo/A-6953-2009 OI Letelier, Ricardo/0000-0003-3376-4026 NR 22 TC 15 Z9 16 U1 0 U2 8 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 14 PY 2007 VL 104 IS 33 BP 13262 EP 13267 DI 10.1073/pnas.0700926104 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 202KE UT WOS:000248899600011 PM 17686987 ER PT J AU Ting, DZY Chang, YC Bandara, SV Gunapala, SD AF Ting, David Z. -Y. Chang, Yia-Chung Bandara, Sumith V. Gunapala, Sarath D. TI Quantum well intrasubband photodetector for far infared and terahertz radiation detection SO APPLIED PHYSICS LETTERS LA English DT Article ID INTERSUBBAND TRANSITIONS; INFRARED PHOTODETECTORS; ABSORPTION AB The authors present a theoretical analysis on the possibility of using the dopant-assisted intrasubband absorption mechanism in quantum wells for normal-incidence far infrared/terahertz radiation detection. The authors describe the proposed concept of the quantum well intrasubband photodetector (QWISP), which is a compact semiconductor heterostructure device compatible with existing GaAs focal-plane array technology, and present theoretical results demonstrating strong normal-incidence absorption and responsivity in the QWISP. (C) 2007 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM david.z.ting@jpl.nasa.gov RI Chang, Yia-Chung/F-4239-2011 NR 18 TC 13 Z9 14 U1 2 U2 9 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 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD AUG 13 PY 2007 VL 91 IS 7 AR 073510 DI 10.1063/1.2770766 PG 3 WC Physics, Applied SC Physics GA 201XT UT WOS:000248866600105 ER PT J AU Mlynczak, MG Marshall, BT Martin-Torres, FJ Russell, JM Thompson, RE Remsberg, EE Gordley, LL AF Mlynczak, Martin G. Marshall, B. Thomas Martin-Torres, F. Javier Russell, James M., III Thompson, R. Earl Remsberg, Ellis E. Gordley, Larry L. TI Sounding of the Atmosphere using Broadband Emission Radiometry observations of daytime mesospheric O-2((1)Delta) 1.27 mu m emission and derivation of ozone, atomic oxygen, and solar and chemical energy deposition rates SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MIDDLE ATMOSPHERE; LOWER THERMOSPHERE; MOLECULAR-OXYGEN; SABER EXPERIMENT; O-2; MODEL; INTENSITIES; EFFICIENCY; 1.27-MU-M; DAYGLOW AB [1] We report observations of the daytime O-2((1)Delta) airglow emission at 1.27 mu m recorded by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the NASAThermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED) satellite. The measured limb radiances are inverted to yield vertical profiles of the volume emission rate of energy from the O-2 molecule. From these emission rates we subsequently derive the mesospheric ozone concentrations using a nonlocal thermodynamic equilibrium (non-LTE) radiative and kinetic model. Rates of energy deposition due to absorption of ultraviolet radiation in the Hartley band of ozone are also derived, independent of knowledge of the ozone abundance and solar irradiances. Atomic oxygen concentrations are obtained from the ozone abundance using photochemical steady state assumptions. Rates of energy deposition due to exothermic chemical reactions are also derived. The data products illustrated here are from a test day (4 July 2002) of SABER Version 1.07 data which are now becoming publicly available. This test day illustrates the high quality of the SABER O-2((1)Delta) airglow and ozone data and the variety of fundamental science questions to which they can be applied. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. G&A Tech Software, Newport News, VA 23606 USA. Analyt Serv & Mat Inc, Hampton, VA 23666 USA. Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. RI Mlynczak, Martin/K-3396-2012; Martin-Torres, Francisco Javier/G-6329-2015 OI Martin-Torres, Francisco Javier/0000-0001-6479-2236 NR 26 TC 23 Z9 23 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 11 PY 2007 VL 112 IS D15 AR D15306 DI 10.1029/2006JD008355 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 202AH UT WOS:000248873400004 ER PT J AU Cremades, H Cyr, OCS Kaiser, ML AF Cremades, H. Cyr, O. C. St. Kaiser, M. L. TI A tool to improve space weather forecasts: Kilometric radio emissions from Wind/WAVES SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID CORONAL MASS EJECTIONS; ARRIVAL TIMES; 1 AU; INTERPLANETARY SHOCKS; ELECTRON-DENSITY; CME; BURSTS; MODELS; WAVES; EARTH AB For decades, space environment forecasters have used the appearance of metric Type II radio emission as a proxy for eruptions in the solar corona. The drift rate of these near-Sun emissions is often turned into a speed, commonly assumed to be that of an MHD shock. However, their utility to forecast shock arrival times has not proved to be conclusive. Metric emissions can be detected by ground-based antennae, while lower-frequency components of these slowly drifting emissions can also be tracked by spacecraft in interplanetary space, as far down in frequency as that of the local plasma frequency. For a spacecraft at L1, this corresponds to about 25 kHz, or an electron density of about 7 cm(-3) in the ambient solar wind. Here we report a recent study that aims to improve the predictions of shock arrival time at L1 by means of the low-frequency emissions detected by WIND/WAVES. This technique, implemented on an extensive sample of hectometric and kilometric type II radio bursts, has yielded promising results. C1 NASA Postdoctral Program, Goddard Space Flight Ctr, Greenbelt, MD USA. [Cyr, O. C. St.; Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cremades, H (reprint author), NASA Postdoctral Program, Goddard Space Flight Ctr, Greenbelt, MD USA. NR 32 TC 15 Z9 15 U1 0 U2 1 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 AUG 11 PY 2007 VL 5 IS 8 AR S08001 DI 10.1029/2007SW000314 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 261JN UT WOS:000253075000001 ER PT J AU Hong, Y Adler, RF Hossain, F Curtis, S Huffman, GJ AF Hong, Yang Adler, Robert F. Hossain, Faisal Curtis, Scott Huffman, George J. TI A first approach to global runoff simulation using satellite rainfall estimation SO WATER RESOURCES RESEARCH LA English DT Article ID LAND-USE CHANGE; SPATIAL VARIABILITY; PRECIPITATION; MODEL; SCALE; RECHARGE; GIS AB Motivated by the recent increasing availability of global remote sensing data for estimating precipitation and describing land surface characteristics, this note reports an approximate assessment of quasi- global runoff computed by incorporating satellite rainfall data and other remote sensing products in a relatively simple rainfall- runoff simulation approach: the Natural Resources Conservation Service ( NRCS) runoff curve number ( CN) method. Using an antecedent precipitation index ( API) as a proxy of antecedent moisture conditions, this note estimates time- varying NRCS- CN values determined by the 5- day normalized API. Driven by a multiyear ( 1998 - 2006) Tropical Rainfall Measuring Mission Multi- satellite Precipitation Analysis, quasi- global runoff was retrospectively simulated with the NRCS- CN method and compared to Global Runoff Data Centre data at global and catchment scales. Results demonstrated the potential for using this simple method when diagnosing runoff values from satellite rainfall for the globe and for medium to large river basins. This work was done with the simple NRCS- CN method as a first- cut approach to understanding the challenges that lie ahead in advancing the satellite- based inference of global runoff. We expect that the successes and limitations revealed in this study will lay the basis for applying more advanced methods to capture the dynamic variability of the global hydrologic process for global runoff monitoring in real time. The essential ingredient in this work is the use of global satellite- based rainfall estimation. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Baltimore, MD 21228 USA. Tennessee Technol Univ, Dept Civil & Environm Engn, Cookeville, TN 38505 USA. E Carolina Univ, Dept Geog, Greenville, NC 27858 USA. Sci Syst & Applicat Inc, Lanham, MD USA. RP Hong, Y (reprint author), Univ Oklahoma, Sch Civil Engn & Environm Sci, Natl Weather Ctr, 120 David L Boren Blvd,Suite 363, Norman, OK 73072 USA. EM yanghong@agnes.gsfc.nasa.gov RI Hong, Yang/D-5132-2009; Curtis, Scott/C-1115-2013; Huffman, George/F-4494-2014; OI Hong, Yang/0000-0001-8720-242X; Huffman, George/0000-0003-3858-8308; Curtis, Scott/0000-0001-9065-8639 NR 39 TC 74 Z9 76 U1 0 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD AUG 11 PY 2007 VL 43 IS 8 AR W08502 DI 10.1029/2006WR005739 PG 8 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 202BV UT WOS:000248877500003 ER PT J AU Saif, B Eegholm, BH Bluth, M Greenfield, P Hack, W Blake, P Keski-Kuha, R North-Morris, M AF Saif, Babak Eegholm, Bente Hoffmann Bluth, Marcel Greenfield, Perry Hack, Warren Blake, Peter Keski-Kuha, Ritva North-Morris, Michael TI Calibration of spatially phase-shifted DSPI for measurement of large structures SO APPLIED OPTICS LA English DT Article AB We present a method for the calibration of a spatially phase-shifted digital speckle pattern interferometer (SPS-DSPI), which was designed and built for the purpose of testing the James Webb space telescope (JWST) optical structures and related technology development structures. The need to measure dynamic deformations of large, diffuse structures to nanometer accuracy at cryogenic temperature is paramount in the characterization of a large diameter space and terrestrial based telescopes. The techniques described herein apply to any situation, in which high accuracy measurement of diffuse structures are required. The calibration of the instrument is done using a single-crystal silicon gauge. The gauge has four islands of different heights that change in a predictable manner as a function of temperature. The SPS-DSPI is used to measure the relative piston between the islands as the temperature of the gauge is changed. The measurement results are then compared with the theoretical changes in the height of the gauge islands. The maximum deviation of the measured rate of change of the relative piston in nm/K from the expected value is 3.3%. (C) 2007 Optical Society of America. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Swales Aerosp, Beltsville, MD 20705 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. 4D Technol, Tucson, AZ 85706 USA. RP Saif, B (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM beegholm@stsci.edu NR 8 TC 5 Z9 5 U1 0 U2 0 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 AUG 10 PY 2007 VL 46 IS 23 BP 5622 EP 5630 DI 10.1364/AO.46.005622 PG 9 WC Optics SC Optics GA 208JJ UT WOS:000249315300011 PM 17694108 ER PT J AU Werdell, PJ Bailey, SW Franz, BA Morel, A McClain, CR AF Werdell, P. Jeremy Bailey, Sean W. Franz, Bryan A. Morel, Andre McClain, Charles R. TI On-orbit vicarious calibration of ocean color sensors using an ocean surface reflectance model SO APPLIED OPTICS LA English DT Article ID DISSOLVED ORGANIC-MATTER; WATER-LEAVING RADIANCE; ATLANTIC TIME-SERIES; NORTH PACIFIC; BIDIRECTIONAL REFLECTANCE; CHLOROPHYLL CONCENTRATION; LIGHT BACKSCATTERING; TEMPERATURE SCANNER; OPTICAL-PROPERTIES; SARGASSO SEA AB Recent advances in global biogeochemical research demonstrate a critical need for long-term ocean color satellite data records of consistent high quality. To achieve that quality, spaceborne instruments require on-orbit vicarious calibration, where the integrated instrument and atmospheric correction system is adjusted using in situ normalized water-leaving radiances, such as those collected by the marine optical buoy (MOBY). Unfortunately, well-characterized time-series of in situ data are scarce for many historical satellite missions, in particular, the NASA coastal zone color scanner (CZCS) and the ocean color and temperature scanner (OCTS). Ocean surface reflectance models (ORMs) accurately reproduce spectra observed in clear marine waters, using only chlorophyll a (C.) as input, a measurement for which long-term in situ time series exist. Before recalibrating CZCS and OCTS using modeled radiances, however, we evaluate the approach with the Sea-viewing Wide-Field-of-view Sensor (SeaWiFS). Using annual C, climatologies as input into an ORM, we derive SeaWiFS vicarious gains that differ from the operational MOBY gains by less than +/- 0.9% spectrally. In the context of generating decadal C-a climate data records, we quantify the downstream effects of using these modeled gains by generating satellite-to-in situ data product validation statistics for comparison with the operational SeaWiFS results. Finally, we apply these methods to the CZCS and OCTS ocean color time series. (C) 2007 Optical Society of America. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Paris 06, Lab Oceanog Villefranche, Villefranche Sur Mer, France. Ctr Natl Rech Sci, Villefranche Sur Mer, France. RP Werdell, PJ (reprint author), NASA, Goddard Space Flight Ctr, 614-2, Greenbelt, MD 20771 USA. EM paul.j.werdell@nasa.gov RI Franz, Bryan/D-6284-2012; Werdell, Jeremy/D-8265-2012; Bailey, Sean/D-3077-2017 OI Franz, Bryan/0000-0003-0293-2082; Bailey, Sean/0000-0001-8339-9763 NR 70 TC 21 Z9 22 U1 0 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD AUG 10 PY 2007 VL 46 IS 23 BP 5649 EP 5666 DI 10.1364/AO.46.005649 PG 18 WC Optics SC Optics GA 208JJ UT WOS:000249315300015 PM 17694112 ER PT J AU Milman, MH Zhai, CP Regehr, M AF Milman, Mark H. Zhai, Chenping Regehr, Martin TI White-light interferometry using a channeled spectrum. I. General models and fringe estimation algorithms SO APPLIED OPTICS LA English DT Article ID STELLAR INTERFEROMETRY; DISPERSION AB Astrometric measurements using stellar interferometry rely on the precise measurement of the central white-light fi-inge to accurately obtain the optical path-length difference of incoming starlight to the two arms of the interferometer. Because of dispersion in the optical system the optical path-length difference is a function of the wavelength of the light and extracting the proper astrometric signatures requires accommodating these effects. One standard approach to stellar interferometry uses a channeled spectrum to determine phases at a number of different wavelengths that are then converted to the path-length delay. Because of throughput considerations these channels are made sufficiently broad so that monochromatic models are inadequate for retrieving the phase/delay information. The presence of dispersion makes the polychromatic modeling problem for phase estimation even more difficult because of its effect on the complex visibility function. We introduce a class of models that rely on just a few spectral and dispersion parameters. A phase-shifting interferometry algorithm is derived that exploits the model structure. Numerical examples are given to illustrate the robustness and precision of the approach. (c) 2007 Optical Society of America. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Milman, MH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mark.h.milman@jpl.nasa.gov NR 21 TC 5 Z9 5 U1 0 U2 0 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 AUG 10 PY 2007 VL 46 IS 23 BP 5853 EP 5865 DI 10.1364/AO.46.005853 PG 13 WC Optics SC Optics GA 208JJ UT WOS:000249315300039 PM 17694135 ER PT J AU Johnson, BR Collins, J Abroe, ME Ade, PAR Bock, J Borrill, J Boscaleri, A de Bernardis, P Hanany, S Jaffe, AH Jones, T Lee, AT Levinson, L Matsumura, T Rabii, B Renbarger, T Richards, PL Smoot, GF Stompor, R Tran, HT Winant, CD Wu, JHP Zuntz, J AF Johnson, B. R. Collins, J. Abroe, M. E. Ade, P. A. R. Bock, J. Borrill, J. Boscaleri, A. de Bernardis, P. Hanany, S. Jaffe, A. H. Jones, T. Lee, A. T. Levinson, L. Matsumura, T. Rabii, B. Renbarger, T. Richards, P. L. Smoot, G. F. Stompor, R. Tran, H. T. Winant, C. D. Wu, J. H. P. Zuntz, J. TI Maxipol: Cosmic microwave background polarimetry using a rotating half-wave plate SO ASTROPHYSICAL JOURNAL LA English DT Article DE polarization ID PROBE WMAP OBSERVATIONS; GALACTIC DUST EMISSION; ANISOTROPY-PROBE; ANGULAR SCALES; 2003 FLIGHT; POLARIZATION; MAXIMA-1; SUBMILLIMETER; RADIATION; INSTRUMENT AB We discuss MAXIPOL, a bolometric balloon-borne experiment designed to measure the E-mode polarization of the cosmic microwave background radiation (CMB). MAXIPOL is the first bolometric CMB experiment to observe the sky using rapid polarization modulation. To build MAXIPOL, the CMB temperature anisotropy experiment MAXIMA was retrofitted with a rotating half-wave plate and a stationary analyzer. We describe the instrument, the observations, the calibration, and the reduction of data collected with 12 polarimeters operating at 140 GHz and with a FWHM beam size of 10'. We present maps of the Q and U Stokes parameters of an 8 deg(2) region of the sky near the star beta UMi. The power spectra computed from these maps give weak evidence for an EE signal. The maximum likelihood amplitude of l(l +/- 1) C-l(EE)/2 pi is 55(-45)(+51) mu K-2 (68%), and the likelihood function is asymmetric and skewed positive such that with a uniform prior the probability that the amplitude is positive is 96%. This result is consistent with the expected concordance Lambda CDM amplitude of 14 mu K-2. The maximum likelihood amplitudes for l(l + 1) C-l(BB)/2 pi and l(l + 1) C-l(EB)/2 pi are -31(-19)(+31) and 18(-34)(+27) mu K-2 ( 68%), respectively, which are consistent with zero. All of the results are for one bin in the range 151 <= l <= 693. Tests revealed no residual systematic errors in the time or map domain. A comprehensive discussion of the analysis of the data is presented in a companion paper. C1 Univ Oxford, Oxford OX1 3RH, England. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, Wales. Jet Propuls Lab, Pasadena, CA 91109 USA. Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA 94720 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. CNR, IFAC, Florence, Italy. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. Imperial Coll, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. Nat Lab, Div Phys, Berkeley, CA 94720 USA. Weizmann Inst Sci, Dept Particle Phys, IL-76100 Rehovot, Israel. Univ Paris 07, Lab AstroParticle Cosmol, Paris, France. Natl Taiwan Univ, Ctr Theoret Sci, Inst Astrophys, Dept Phys, Taipei 10617, Taiwan. RP Johnson, BR (reprint author), Univ Oxford, S Parks Rd, Oxford OX1 3RH, England. RI Jaffe, Andrew/D-3526-2009; OI de Bernardis, Paolo/0000-0001-6547-6446; WU, JIUN-HUEI/0000-0001-9608-7662 NR 38 TC 38 Z9 38 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 AUG 10 PY 2007 VL 665 IS 1 BP 42 EP 54 DI 10.1086/518105 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700004 ER PT J AU Wu, JHP Zuntz, J Abroe, ME Ade, PAR Bock, J Borrill, J Collins, J Hanany, S Jaffe, AH Johnson, BR Jones, T Lee, AT Matsumura, T Rabii, B Renbarger, T Richards, PL Smoot, GF Stompor, R Tran, HT Winant, CD AF Wu, J. H. P. Zuntz, J. Abroe, M. E. Ade, P. A. R. Bock, J. Borrill, J. Collins, J. Hanany, S. Jaffe, A. H. Johnson, B. R. Jones, T. Lee, A. T. Matsumura, T. Rabii, B. Renbarger, T. Richards, P. L. Smoot, G. F. Stompor, R. Tran, H. T. Winant, C. D. TI Maxipol: Data analysis and results SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; methods : data analysis; polarization ID MICROWAVE BACKGROUND ANISOTROPY; ANGULAR SCALES; POWER SPECTRUM; POLARIZATION; MAXIMA-1; BOOMERANG; PROBE; WMAP AB We present results from and the analysis of data from MAXIPOL, a balloon- borne experiment designed to measure the polarization in the cosmic microwave background (CMB). MAXIPOL is the first CMB experiment to obtain results using a rotating half-wave plate as a rapid polarization modulator. We report results from observations of a sky area of 8 deg(2) with 100 resolution, providing information up to l similar to 700. We use a maximum likelihood method to estimate maps of the Q and U Stokes parameters from the demodulated time streams, and then both Bayesian and frequentist approaches to compute the EE, EB, and BB power spectra. Detailed formalisms of the analyses are given. We give results for the amplitude of the power spectra assuming different shape functions within the l bins, with and without a prior C-l(EB) = C-l(BB) = 0, and with and without inclusion of calibration uncertainty. We show results from systematic tests including differencing of maps, analyzing sky areas of different sizes, assessing the influence of leakage from temperature to polarization, and quantifying the Gaussianity of the maps. We find no evidence for systematic errors. The Bayesian analysis gives weak evidence for an EE signal. The EE power is 55(-45)(+51) mu K-2 at the 68% confidence level for l = 151-693. Its likelihood function is asymmetric and skewed positive such that with a uniform prior the probability of a positive EE power is 96%. The powers of EB and BB signals at the 68% confidence level are 18(-34)(+27) and 31(-19)(+31) mu K-2, respectively, and thus consistent with zero. The upper limit of the BB-mode at the 95% confidence level is 9.5 mu K. Results from the frequentist approach are in agreement within statistical errors. These results are consistent with the current concordance Lambda CDM model. C1 Natl Taiwan Univ, Inst Astrophys, Ctr Theoret Sci, Dept Phys, Taipei 10617, Taiwan. Imperial Coll, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3Y, S Glam, Wales. Jet Propuls Lab, Pasadena, CA 91109 USA. Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA 94720 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Oxford, Oxford OX1 3RH, England. Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. Univ Paris 07, Lab AstroParticule Cosmol, Paris, France. RP Wu, JHP (reprint author), Natl Taiwan Univ, Inst Astrophys, Ctr Theoret Sci, Dept Phys, Taipei 10617, Taiwan. RI Jaffe, Andrew/D-3526-2009; OI WU, JIUN-HUEI/0000-0001-9608-7662 NR 30 TC 44 Z9 44 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 AUG 10 PY 2007 VL 665 IS 1 BP 55 EP 66 DI 10.1086/518112 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700005 ER PT J AU Markowitz, A Takahashi, T Watanabe, S Nakazawa, K Fukazawa, Y Kokubun, M Makishima, K Awaki, H Bamba, A Isobe, N Kataoka, J Madejski, G Mushotzky, R Okajima, T Ptak, A Reeves, JN Ueda, Y Yamasaki, T Yaqoob, T AF Markowitz, A. Takahashi, T. Watanabe, S. Nakazawa, K. Fukazawa, Y. Kokubun, M. Makishima, K. Awaki, H. Bamba, A. Isobe, N. Kataoka, J. Madejski, G. Mushotzky, R. Okajima, T. Ptak, A. Reeves, J. N. Ueda, Y. Yamasaki, T. Yaqoob, T. TI The Suzaku observation of the nucleus of the radio-loud active galaxy Centaurus A: Constraints on abundances of the accreting material SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 5128); X-rays : galaxies ID X-RAY-EMISSION; ADVECTION-DOMINATED ACCRETION; XMM-NEWTON OBSERVATIONS; NGC 5128; METALLICITY DISTRIBUTION; BOARD SUZAKU; HALO STARS; BLACK-HOLE; FR-I; CHANDRA AB A Suzaku observation of the nucleus of the radio-loud AGN Centaurus A in 2005 has yielded a broadband spectrum spanning 0.3-250 keV. The net exposure times after screening were 70 ks per X-ray Imaging Spectrometer (XIS) camera, 60.8 ks for the Hard X- ray Detector (HXD) PIN, and 17.1 ks for the HXD GSO. The hard X- rays are fit by two power laws of the same slope, absorbed by columns of 1.5 and 7 x 10(23) cm(-2), respectively. The spectrum is consistent with previous suggestions that the power-law components are X- ray emission from the subparsec VLBI jet and from Bondi accretion at the core, but it is also consistent with a partial-covering interpretation. The soft band is dominated by thermal emission from the diffuse plasma and is fit well by a two-temperature VAPEC model, plus a third power-law component to account for scattered nuclear emission, jet emission, and emission from X- ray binaries and other point sources. Narrow fluorescent emission lines from Fe, Si, S, Ar, Ca, and Ni are detected. The Fe K proportional to line width yields a 200 lt-day lower limit on the distance from the black hole to the line-emitting gas. Fe, Ca, and S K-shell absorption edges are detected. Elemental abundances are constrained via absorption edge depths and strengths of the fluorescent and diffuse plasma emission lines. The high metallicity ([Fe/H] = +0.1) of the circumnuclear material suggests that it could not have originated in the relatively metal-poor outer halo unless enrichment by local star formation has occurred. Relative abundances are consistent with enrichment from Type II and Ia supernovae. C1 NASA, Goddard Space Flight Ctr, X Ray Astrophys Lab, Greenbelt, MD 20771 USA. Inst Space & Astronaut Sci, JAXA, Sagamihara, Kanagawa 229, Japan. Hiroshima Univ, Dept Phys, Higashihiroshima 739, Japan. Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo, Japan. Inst Phys & Chem Res, Wako, Saitama 35101, Japan. Ehime Univ, Fac Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. Tokyo Inst Technol, Dept Phys, Tokyo 152, Japan. Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Kyoto Univ, Dept Astron, Kyoto 606, Japan. RP Markowitz, A (reprint author), NASA, Goddard Space Flight Ctr, X Ray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. EM agm@milkyway.gsfc.nasa.gov RI Ptak, Andrew/D-3574-2012; XRAY, SUZAKU/A-1808-2009 NR 65 TC 41 Z9 41 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2007 VL 665 IS 1 BP 209 EP 224 DI 10.1086/519271 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700015 ER PT J AU Chary, RR Teplitz, HI Dickinson, ME Koo, DC Le Floc'h, E Marcillac, D Papovich, C Stern, D AF Chary, Ranga-Ram Teplitz, Harry I. Dickinson, Mark E. Koo, David C. Le Floc'h, Emeric Marcillac, Delphine Papovich, Casey Stern, Daniel TI Hubble ultra deep field-jd2: Mid-infrared evidence for a z similar to 2 luminous infrared galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; early universe; galaxies : evolution; galaxies : individual (HUDF-JD2) ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; EXTREMELY RED OBJECTS; HIGH-REDSHIFT; SPECTROGRAPH; CAMERA; DUST; CALIBRATION; RESOLUTION; SAMPLE AB The Hubble Ultra Deep Field source JD2 presented in Mobasher et al. is an unusual galaxy that is very faint at all wavelengths shortward of 1.1 mu m. Photometric redshift fits to data between 0.4 and 8 mu m yield a significant probability that it is an extremely massive galaxy at z similar to 6: 5. In this paper we present new photometry at 16 and 22 mu m from Spitzer Infrared Spectrograph (IRS) peak-up imaging of the Great Observatories Origins Deep Survey ( GOODS) fields. We find that the spectral energy distribution shows a factor of similar to 4 rise in flux density between the 16 and 22 mu m bandpass, which is most likely due to the entrance of polycyclic aromatic hydrocarbon emission features into the 22 and 24 mu m passbands. The flux ratio between these bandpasses can be best fit by a z 1: 7 luminous infrared galaxy with a bolometric luminosity of ( 2 6); 1011 L-circle dot corresponding to a star formation rate of 80 M-circle dot yr(-1). The predicted flux density values at other longer wavelengths are below the detection limits of current instrumentation, but such sources could potentially be detected in lensed submillimeter surveys. Reevaluation of the optical/near-infrared photometry continues to favor z > 6 photometric redshift solutions, but we argue that the consistency of the multiwavelength parameters of this galaxy with other dusty starbursts favor the z similar to 2 mid-infrared photometric redshift. The data presented here provide evidence that optically undetected near-infrared sources that are detected at 24 mu m are most likely dusty, starburst galaxies at a redshift of z similar to 2 with stellar masses > 10(10) M-circle dot. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Inst Astron, Honolulu, HI USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Jet Prop Lab, Pasadena, CA 91109 USA. RP Chary, RR (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM rchary@caltech.edu NR 29 TC 21 Z9 21 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 AUG 10 PY 2007 VL 665 IS 1 BP 257 EP 264 DI 10.1086/519243 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700020 ER PT J AU Kogut, A Dunkley, J Bennett, CL Dore, O Gold, B Halpern, M Hinshaw, G Jarosik, N Komatsu, E Nolta, MR Odegard, N Page, L Spergel, DN Tucker, GS Weiland, JL Wollack, E Wright, EL AF Kogut, A. Dunkley, J. Bennett, C. L. Dore, O. Gold, B. Halpern, M. Hinshaw, G. Jarosik, N. Komatsu, E. Nolta, M. R. Odegard, N. Page, L. Spergel, D. N. Tucker, G. S. Weiland, J. L. Wollack, E. Wright, E. L. TI Three-year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Foreground polarization SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; dust, extinction; polarization; radio continuum : ISM ID MAGNETIC-FIELDS; RADIO-EMISSION; DUST GRAINS; GALAXIES; SPECTRUM; NGC-891; MAPS AB We present a full-sky model of polarized Galactic microwave emission based on 3 years of observations by the Wilkinson Microwave Anisotropy Probe (WMAP) at frequencies from 23 to 94 GHz. The model compares maps of the Stokes Q and U components from each of the five WMAP frequency bands in order to separate synchrotron from dust emission, taking into account the spatial and frequency dependence of the synchrotron and dust components. This simple two-component model of the interstellar medium accounts for at least 97% of the polarized emission in the WMAP maps of the microwave sky. Synchrotron emission dominates the polarized foregrounds at frequencies below 50 GHz, and is comparable to the dust contribution at 65 GHz. The spectral index of the synchrotron component, derived solely from polarization data, is -3.2 averaged over the full sky, with a modestly flatter index on the Galactic plane. The synchrotron emission has mean polarization fraction 2% -4% in the Galactic plane and rising to over 20% at high latitude, with prominent features such as the north Galactic spur more polarized than the diffuse component. Thermal dust emission has polarization fraction 1% near the Galactic center, rising to 6% at the anticenter. Diffuse emission from high-latitude dust is also polarized with mean fractional polarization 0.036 +/- 0.011. C1 Princeton Univ, NASA, Goddard Space Flight Ctr, WMAP Sci Team, Princeton, NJ 08544 USA. Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. Univ Texas, Dept Astron, Vancouver, BC V6T 1Z1, Canada. Brown Univ, Dept Phys, Providence, RI 02912 USA. Univ Calif Los Angeles, PAB 3 909, Los Angeles, CA 90095 USA. RP Kogut, A (reprint author), Princeton Univ, NASA, Goddard Space Flight Ctr, WMAP Sci Team, Princeton, NJ 08544 USA. EM alan.j.kogut@nasa.gov RI Kogut, Alan/D-6293-2012; Komatsu, Eiichiro/A-4361-2011; Spergel, David/A-4410-2011; Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 NR 22 TC 76 Z9 76 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2007 VL 665 IS 1 BP 355 EP 362 DI 10.1086/519754 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700026 ER PT J AU Stutz, AM Bieging, JH Rieke, GH Shirley, YL Balog, Z Gordon, KD Green, EM Keene, J Kelly, BC Rubin, M Werner, MW AF Stutz, Amelia M. Bieging, John H. Rieke, George H. Shirley, Yancy L. Balog, Zoltan Gordon, Karl D. Green, Elizabeth M. Keene, Jocelyn Kelly, Brandon C. Rubin, Mark Werner, Michael W. TI Spitzer observations of a 24 mu m shadow: BOK globule CB 190 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared : ISM; ISM : globules; ISM : individual ([CB88] 190) ID MULTIBAND IMAGING PHOTOMETER; INTERSTELLAR DUST GRAINS; MAGNETIC-FIELD SUPPORT; MOLECULAR CLOUD CORES; MASS STAR-FORMATION; AMBIPOLAR-DIFFUSION; INFRARED EXTINCTION; MILKY-WAY; FRAGMENTATION; INSTABILITY AB We present Spitzer observations of the dark globule CB 190 (LDN 771). We observe a roughly circular 24 mu m shadow with a 70" radius. The extinction profile of this shadow matches the profile derived from 2MASS photometry at the outer edges of the globule and reaches a maximum of similar to 32 visual magnitudes at the center. The corresponding mass of CB 190 is similar to 10M .. Our (CO)-C-12 and (CO)-C-13 J = 2-1 data over a 10' x 10' region centered on the shadow show a temperature similar to 10 K. The thermal continuum indicates a similar temperature for the dust. The molecular data also show evidence of freezeout onto dust grains. We estimate a distance to CB 190 of 400 pc using the spectroscopic parallax of a star associated with the globule. Bonnor-Ebert fits to the density profile, in conjunction with this distance, yield xi(max =) 7.2, indicating that CB 190 may be unstable. The high temperature (56 K) of the best-fit Bonnor-Ebert model is in contradiction with the CO and thermal continuum data, leading to the conclusion that the thermal pressure is not enough to prevent free-fall collapse. We also find that the turbulence in the cloud is inadequate to support it. However, the cloud may be supported by the magnetic field, if this field is at the average level for dark globules. Since the magnetic field will eventually leak out through ambipolar diffusion, it is likely that CB 190 is collapsing or in a late precollapse stage. C1 Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Stutz, AM (reprint author), Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. EM astutz@as.arizona.edu NR 51 TC 14 Z9 14 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2007 VL 665 IS 1 BP 466 EP 477 DI 10.1086/519488 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700035 ER PT J AU Ardila, DR Golimowski, DA Krist, JE Clampin, M Ford, HC Illingworth, GD AF Ardila, D. R. Golimowski, D. A. Krist, J. E. Clampin, M. Ford, H. C. Illingworth, G. D. TI Hubble Space Telescope advanced camera for surveys coronagraphic observations of the dust surrounding HD 100546 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : protoplanetary disks; stars : imaging; stars : individual (HD 100546); stars : pre-main-sequence ID HERBIG-AE STAR; TAURI CIRCUMBINARY DISK; SPECTRAL ENERGY-DISTRIBUTIONS; MODEL SCATTERING ENVELOPES; YOUNG STELLAR OBJECTS; KUIPER-BELT OBJECTS; CIRCUMSTELLAR DISK; AE/BE STARS; HD 100546; DEBRIS DISK AB We present HSTACS coronagraphic observations of HD 100546, a B9.5 star, 103 pc away from the Sun, taken in the F435W, F606W, and F814W bands. Scattered light is detected up to 1400 from the star. The observations are consistent with the presence of an extended flattened nebula with the same inclination as the inner disk. The well-known "spiral arms" are clearly observed and trail the rotating disk material. Weaker arms never before reported are also seen. The interarm space becomes brighter, but the structures become more neutral in color at longer wavelengths, which is not consistent with models that assume that they are due to the effects of a warped disk. Along the major disk axis, the colors of the scattered light relative to the star are Delta( F435W - F606W) approximate to 0.0-0.2 mag and Delta( F435W - F814W) approximate to 0.5-1 mag. To explain these colors, we explore the role of asymmetric scattering, reddening, and large minimum sizes on ISM-like grains. We conclude that each of these hypotheses by itself cannot explain the colors. The disk colors are similar to those derived for Kuiper Belt objects, suggesting that the same processes responsible for their colors may be at work here. We argue that we are observing only the geometrically thick, optically thin envelope of the disk, while the optically thick disk responsible for the far-IR emission is undetected. The observed spiral arms are then structures on this envelope. The colors indicate that the extended nebulosity is not a remnant of the infalling envelope but reprocessed disk material. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. RP Ardila, DR (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM ardila@ipac.caltech.edu RI Clampin, mark/D-2738-2012 NR 88 TC 42 Z9 42 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2007 VL 665 IS 1 BP 512 EP 534 DI 10.1086/519296 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700038 ER PT J AU Krimm, HA Granot, J Marshall, FE Perri, M Barthelmy, SD Burrows, DN Gehrels, N Meszaros, P Morris, D AF Krimm, H. A. Granot, J. Marshall, F. E. Perri, M. Barthelmy, S. D. Burrows, D. N. Gehrels, N. Meszaros, P. Morris, D. TI GRB 060714: No clear dividing line between prompt emission and X-ray flares SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID AFTERGLOW LIGHT CURVES; BURST AFTERGLOWS; REFRESHED SHOCKS; GRB AFTERGLOWS; ENGINE ACTIVITY; TELESCOPE; VARIABILITY; LONG; GRB-021004; ENERGETICS AB The long gamma-ray burst GRB 060714 was observed to exhibit a series of five X-ray flares beginning similar to 70 s after the burst trigger T-0 and continuing until similar to T-0 + 200 s. The first two flares were detected by the Burst Alert Telescope (BAT) on the Swift satellite, before Swift had slewed to the burst location, while the last three flares were strongly detected by the X-Ray Telescope (XRT) but only weakly detected by the BAT. This burst provides an unusual opportunity to track a complete sequence of flares over a wide energy range. The flares were very similar in their light curve morphology, showing power-law rise and fall components, and in most cases significant substructure. The flares also showed strong evolution with time, both spectrally and temporally. The small timescale and large amplitude variability observed are incompatible with an external shock origin for the flares, and support instead late-time sporadic activity either of the central source or of localized dissipation events within the outflow. We show that the flares in GRB 060714 cannot be the result of internal shocks in which the contrast in the Lorentz factor of the colliding shells is very small, and that this mechanism faces serious difficulties in most Swift GRBs. The morphological similarity of the flares and the prompt emission and the gradual and continual evolution of the flares with time makes it difficult and arbitrary to draw a dividing line between the prompt emission and the flares. C1 NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Stanford Univ, KIPAC, Stanford, CA 94309 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. ASI Sci Data Ctr, I-00044 Frascati, Italy. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RP Krimm, HA (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; OI Perri, Matteo/0000-0003-3613-4409 NR 74 TC 26 Z9 26 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2007 VL 665 IS 1 BP 554 EP 568 DI 10.1086/519019 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700040 ER PT J AU Troja, E Cusumano, G O'Brien, PT Zhang, B Sbarufatti, B Mangano, V Willingale, R Chincarini, G Osborne, JP Marshall, FE Burrows, DN Campana, S Gehrels, N Guidorzi, C Krimm, HA La Parola, V Liang, EW Mineo, T Moretti, A Page, KL Romano, P Tagliaferri, G Zhang, BB Page, MJ Schady, P AF Troja, E. Cusumano, G. O'Brien, P. T. Zhang, B. Sbarufatti, B. Mangano, V. Willingale, R. Chincarini, G. Osborne, J. P. Marshall, F. E. Burrows, D. N. Campana, S. Gehrels, N. Guidorzi, C. Krimm, H. A. La Parola, V. Liang, E. W. Mineo, T. Moretti, A. Page, K. L. Romano, P. Tagliaferri, G. Zhang, B. B. Page, M. J. Schady, P. TI Swift observations of GRB 070110: An extraordinary X-ray afterglow powered by the central engine SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; X-rays : individual (GRB 070110) ID CONTINUOUS ENERGY INJECTION; GAMMA-RAY; BURST AFTERGLOWS; PARAMETER-ESTIMATION; MILLISECOND PULSARS; LIGHT CURVES; DUST; FLARES; TELESCOPE; EMISSION AB We present a detailed analysis of Swift multiwavelength observations of GRB 070110 and its remarkable afterglow. The early X-ray light curve, interpreted as the tail of the prompt emission, displays a spectral evolution already seen in other gamma-ray bursts. The optical afterglow shows a shallow decay up to similar to 2 days after the burst, which is not consistent with standard afterglow models. The most intriguing feature is a very steep decay in the X-ray flux at similar to 2 x 10(4) s after the burst, ending an apparent plateau. The abrupt drop of the X-ray light curve rules out an external shock as the origin of the plateau in this burst and implies long-lasting activity of the central engine. The temporal and spectral properties of the plateau phase point toward a continuous central engine emission rather than the episodic emission of X-ray flares. We suggest that the observed X-ray plateau is powered by a spinning-down central engine, possibly a millisecond pulsar, which dissipates energy at an internal radius before depositing energy into the external shock. C1 Ist Astrofis Spaziale & Fis Cosmc, Sezione Palermo, INAF, I-90146 Palermo, Italy. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Palermo, Dipartimento Sci Fisiche & Astron, Sezione Astron, I-90134 Palermo, Italy. Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. Univ Milan, Dipartimento Fis, I-20126 Milan, Italy. INAF Osservat Astron Brera, I-23807 Merate, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Univ Space Res Assoc, Columbia, MD 20144 USA. Guangxi Univ, Dept Phys, Nanning 530004, Peoples R China. Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, Kunming, Peoples R China. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Troja, E (reprint author), Ist Astrofis Spaziale & Fis Cosmc, Sezione Palermo, INAF, Via Ugo Malfa 153, I-90146 Palermo, Italy. RI Gehrels, Neil/D-2971-2012; Zhang, Binbin/C-9035-2013; OI Zhang, Binbin/0000-0003-2002-116X; Mineo, Teresa/0000-0002-4931-8445; Cusumano, Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315; La Parola, Valentina/0000-0002-8087-6488; Sbarufatti, Boris/0000-0001-6620-8347; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 70 TC 112 Z9 113 U1 0 U2 8 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 AUG 10 PY 2007 VL 665 IS 1 BP 599 EP 607 DI 10.1086/519450 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700042 ER PT J AU Stute, M Sahai, R AF Stute, Matthias Sahai, Raghvendra TI Hydrodynamical simulations of the jet in the symbiotic star MWC 560. III. Application to X-ray jets in symbiotic stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : symbiotic; circumstellar matter; hydrodynamics; ISM : jets and outflows; methods : numerical; X-rays : ISM ID SYSTEM CH-CYGNI; R-AQUARII; ACCRETION DISKS; EMISSION; ULTRAVIOLET; OUTFLOW; MOTION; FLOWS; MODEL; WINDS AB In Papers I and II in this series, we presented hydrodynamical simulations of jet models with parameters representative of the symbiotic system MWC 560. These were simulations of a pulsed, initially underdense jet in a high-density ambient medium. Since the pulsed emission of the jet creates internal shocks and since the jet velocity is very high, the jet bow shock and the internal shocks are heated to high temperatures and should therefore emit X-ray radiation. In this paper, we investigate in detail the X-ray properties of the jets in our models. We have focused our study on the total X-ray luminosity and its temporal variability, the resulting spectra, and the spatial distribution of the emission. Temperature and density maps from our hydrodynamical simulations with radiative cooling presented in the second paper are used, together with emissivities calculated with the atomic database ATOMDB. The jets in our models show extended and variable X-ray emission, which can be characterized as a sum of hot and warm components with temperatures that are consistent with observations of CHCyg and R Aqr. The X-ray spectra of our model jets show emission-line features that correspond to observed features in the spectra of CH Cyg. The innermost parts of our pulsed jets show iron line emission in the 6.4-6.7 keV range, which may explain such emission from the central source in R Aqr. We conclude that MWC 560 should be detectable with Chandra or XMM-Newton, and such X-ray observations will prove crucial for understanding jets in symbiotic stars. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Stute, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Matthias.Stute@jpl.nasa.gov NR 34 TC 10 Z9 10 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 AUG 10 PY 2007 VL 665 IS 1 BP 698 EP 706 DI 10.1086/518930 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700052 ER PT J AU Piana, M Massone, AM Hurford, GJ Prato, M Emslie, AG Kontar, EP Schwartz, RA AF Piana, Michele Massone, Anna Maria Hurford, G. J. Prato, Marco Emslie, A. Gordon Kontar, Eduard P. Schwartz, Richard A. TI Electron flux spectral imaging of solar flares through regularized analysis of hard X-ray source visibilities SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; Sun : flares; Sun : X-rays, gamma rays; techniques : image processing; techniques : spectroscopic ID 2002 JULY 23; GAMMA-RAY; RHESSI AB We introduce a new method for imaging spectroscopy analysis of hard X-ray emission during solar flares. The method avoids the " traditional'' noise-sensitive step of stacking independent images made in different count-based energy intervals. Rather, it involves regularized inversion of the count visibility spectra ( i.e., the two-dimensional spatial Fourier transforms of the spectral image) to obtain smoothed (regularized) forms of the corresponding electron visibility spectra. Application of conventional visibility-based imaging algorithms then yields images of the electron flux that vary smoothly with energy. We apply the method to a solar flare observed on 2002 February 20 by the RHESSI instrument. The event is characterized by two bright footpoints with a more diffuse emission between them. Analysis of the regularized electron flux images reveals that the electron flux spectra at the footpoints are systematically harder than those in the region between the footpoints and that the observed degree of hardening is consistent with that produced by Coulomb collisions between an acceleration site high in the corona and the dense chromospheric footpoint regions. C1 Univ Verona, Dipartimento Informat, I-37134 Verona, Italy. CNR, INFM, LAMIA, I-16145 Genoa, Italy. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Modena & Reggio Emilia, Dipartimento Matemat, I-41100 Modena, Italy. Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. Catholic Univ, NASA, Goddard Space Flight Ctr, LSSP, Greenbelt, MD 20771 USA. RP Piana, M (reprint author), Univ Verona, Dipartimento Informat, Ca Vignal 2,Strada Le Grazie, I-37134 Verona, Italy. EM michele.piana@univr.it; massone@ge.infm.it; ghurford@ssl.berkeley.edu; marco.prato@unimo.it; gordon.emslie@okstate.edu; eduard@astro.gla.ac.uk; richard.schwartz@gsfc.nasa.gov RI Kontar, Eduard/B-7897-2008; Prato, Marco/G-4096-2011; piana, michele/H-9376-2015; OI Kontar, Eduard/0000-0002-8078-0902; Prato, Marco/0000-0002-7327-3347; PIANA, MICHELE/0000-0003-1700-991X NR 15 TC 33 Z9 33 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2007 VL 665 IS 1 BP 846 EP 855 DI 10.1086/519518 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DF UT WOS:000248675700066 ER PT J AU Eriksen, HK Huey, G Banday, AJ Gorski, KM Jewell, JB O'Dwyer, IJ Wandelt, BD AF Eriksen, H. K. Huey, Greg Banday, A. J. Gorski, K. M. Jewell, J. B. O'Dwyer, I. J. Wandelt, B. D. TI Bayesian analysis of the low-resolution polarized 3 year WMAP sky maps SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; methods : numerical ID MICROWAVE; POWER AB We apply a previously developed Gibbs sampling framework to the foreground- corrected 3 yr WMAP polarization data and compute the power spectrum and residual foreground template amplitude posterior distributions. We first analyze the co- added Q- and V- band data, and compare our results to the likelihood code published by the WMAP team. We find good agreement, and thus verify the numerics and data- processing steps of both approaches. However, we also analyze the Q- and V- band data separately, allowing for nonzero EB cross-correlations and including two individual foreground template amplitudes tracing synchrotron and dust emission. In these analyses, we find tentative evidence of systematics: The foreground tracers correlate with each of the Q- and V- band sky maps individually, although not with the co- added QV map; there is a noticeable negative EB cross- correlation at in the V- band map; and finally, when relaxing the constraints on EB and BB, l <= 16 noticeable differences are observed between the marginalized band powers in the Q and V bands. Further studies of these features are imperative, given the importance of the low- EE spectrum on the optical depth of reionization l tau and the spectral index of scalar perturbations n(s). C1 Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Pasadena, CA 91125 USA. Max Planck Inst Astrophys, D-85741 Munich, Germany. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Eriksen, HK (reprint author), Univ Oslo, Inst Theoret Astrophys, PO Box 1029 Blindern, N-0315 Oslo, Norway. EM h.k.k.eriksen@astro.uio.no NR 13 TC 23 Z9 23 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2007 VL 665 IS 1 BP L1 EP L4 DI 10.1086/521191 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DJ UT WOS:000248676100001 ER PT J AU Yeh, KS AF Yeh, Kao-San TI The streamline subgrid integration method: I. Quasi-monotonic second-order transport schemes SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE conservative; monotonic; positive-definite; semi-lagrangian; finite-volume; transport; multidimensional; lcosahedral; geodesic ID BAROTROPIC VORTICITY EQUATION; SHALLOW-WATER EQUATIONS; CONSERVATION-LAWS; MODELS; SPHERE AB A new finite-volume method has been developed for conservative and monotonic transport in multiple dimensions without any sort of dimension splitting to emphasize the space-time integrity of the fluid system. The streamline subgrid integration (SSI) method is a combination of the semi-Lagrangian and the finite-volume methods with generalized multidimensional subgrid distributions. Second-order transport schemes are constructed in two dimensions, and their extensions to three dimensions are also discussed. Spurious divergence is rigorously controlled with Lagrangian control volumes, monotonicity is well preserved for both compressible and incompressible flows, and positive-definiteness is always guaranteed. The accuracy and the numerical properties of these schemes are evaluated with both continuous and discontinuous solutions in flows of rigid motion and incompressible deformation where analytic solutions are available. Icosahedral geodesic grids are selected to demonstrate the general nature of the SSI method in spherical geometry that the numerical solutions are virtually not affected by the irregularity of grid structure. We have found that the numerical solutions converge quickly to the analytic solutions, and the SSI second-order schemes are relatively more beneficial for high-resolution applications. (c) 2007 Elsevier Inc. All rights reserved. C1 [Yeh, Kao-San] Univ Maryland, Baltimore Cty, MD 21250 USA. RP Yeh, KS (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA. EM kYeh@postit.gsfc.nasa.gov NR 20 TC 12 Z9 12 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 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD AUG 10 PY 2007 VL 225 IS 2 BP 1632 EP 1652 DI 10.1016/j.jcp.2007.02.033 PG 21 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 292ZL UT WOS:000255304500023 ER PT J AU Kanevsky, A Carpenter, MH Gottlieb, D Hesthaven, JS AF Kanevsky, Alex Carpenter, Mark H. Gottlieb, David Hesthaven, Jan S. TI Application of implicit-explicit high order Runge-Kutta methods to discontinuous-Galerkin schemes SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE high-order; discontinuous Galerkin finite element method (DGFEM); implicit-explicit (IMEX) method; Navier-Stokes equations ID PARTIAL-DIFFERENTIAL-EQUATIONS; CONTROL-THEORETIC TECHNIQUES; NAVIER-STOKES EQUATIONS; STEPSIZE SELECTION; NUMERICAL-SOLUTION; ELEMENT METHOD; FLOW AB Despite the popularity of high-order explicit Runge-Kutta (ERK) methods for integrating semi-discrete systems of equations, ERK methods suffer from severe stability-based time step restrictions for very stiff problems. We implement a discontinuous Galerkin finite element method (DGFEM) along with recently introduced high-order implicit-explicit Runge-Kutta (IMEX-RK) schemes to overcome geometry-induced stiffness in fluid-flow problems. The IMEX algorithms solve the non-stiff portions of the domain using explicit methods, and isolate and solve the more expensive stiff portions using an L-stable, stiffly-accurate explicit, singly diagonally implicit Runge-Kutta method (ESDIRK). Furthermore, we apply adaptive time-step controllers based on the embedded temporal error predictors. We demonstrate in a number of numerical test problems that IMEX methods in conjunction with efficient preconditioning become more efficient than explicit methods for systems exhibiting high levels of grid-induced stiffness. (c) 2007 Elsevier Inc. All rights reserved. C1 [Kanevsky, Alex; Gottlieb, David; Hesthaven, Jan S.] Brown Univ, Div Appl Math, Providence, RI 02912 USA. [Carpenter, Mark H.] NASA, Langley Res Ctr, Aeronaut & Aeroacoust Methods Branch, Hampton, VA 23681 USA. RP Kanevsky, A (reprint author), Brown Univ, Div Appl Math, Box F, Providence, RI 02912 USA. EM kanevsky@dam.brown.edu; Mark.H.Carpenter@nasa.gov; dig@dam.brown.edu; Jaii.Hesthaven@Brown.edu RI Hesthaven, Jan/A-7602-2009 OI Hesthaven, Jan/0000-0001-8074-1586 NR 44 TC 59 Z9 59 U1 1 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD AUG 10 PY 2007 VL 225 IS 2 BP 1753 EP 1781 DI 10.1016/j.jcp.2007.02.021 PG 29 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 292ZL UT WOS:000255304500029 ER PT J AU Fairfield, DH Kuznetsova, MM Mukai, T Nagai, T Gombosi, TI Ridley, AJ AF Fairfield, D. H. Kuznetsova, M. M. Mukai, T. Nagai, T. Gombosi, T. I. Ridley, A. J. TI Waves on the dusk flank boundary layer during very northward interplanetary magnetic field conditions: Observations and simulation SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID KELVIN-HELMHOLTZ INSTABILITY; GLOBAL MAGNETOSPHERIC OSCILLATIONS; 10-11 JANUARY 1997; SOLAR-WIND; GEOTAIL OBSERVATIONS; MAGNETOSHEATH FLOW; CONVECTIVE INSTABILITY; SUBSOLAR MAGNETOPAUSE; MAGNETOTAIL BOUNDARY; CLUSTER OBSERVATIONS AB The Geotail spacecraft made an inbound passage perpendicular to the dusk equatorial magnetopause on 1 August 1998 when the interplanetary magnetic field had been very northward for more than 10 hours. As the spacecraft moved through the low- latitude boundary layer, it detected waves with similar to 3 min period that caused transitions between cool dense magnetosheath plasma and mixed magnetosheath and magnetosphere plasmas. A region of highly fluctuating magnetic fields with variations up to 50 nT/ s was observed on leaving the magnetosheath plasma but not on its return to this region. This observation suggests that the boundary region is not laminar but more likely consists of Kelvin-Helmholtz vortices. Such fluctuations are probably caused by twisting of the field by the vortices, and they could be important in transporting plasma to the magnetosphere where densities of 5/ cc were observed. A global MHD simulation of the event reproduced the observed low- frequency waves, their counterclockwise polarization, and a region of high- velocity magnetosheath flow outside the magnetopause. This flow was associated with a decreased density and increased field strength which are characteristics of a plasma depletion layer. When Geotail moved further inward into the magnetosphere, it detected waves that are probably the magnetotail vortices which had been detected earlier by the ISEE spacecraft. C1 NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. Inst Space & Astronaut Sci, Kanagawa 229, Japan. Tokyo Inst Technol, Tokyo 152, Japan. RP Fairfield, DH (reprint author), NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. EM donald.fairfield@nasa.gov RI Ridley, Aaron/F-3943-2011; Gombosi, Tamas/G-4238-2011; Kuznetsova, Maria/F-6840-2012 OI Ridley, Aaron/0000-0001-6933-8534; Gombosi, Tamas/0000-0001-9360-4951; NR 65 TC 38 Z9 40 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 9 PY 2007 VL 112 IS A8 AR A08206 DI 10.1029/2006JA012052 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 202BG UT WOS:000248875900002 ER PT J AU Adesokan, AA Chaban, GM Dopfer, O Gerber, RB AF Adesokan, Adeyemi A. Chaban, Galina M. Dopfer, Otto Gerber, R. Benny TI Vibrational spectroscopy of protonated imidazole and its complexes with water molecules: Ab initio anharmonic calculations and experiments SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID INFRARED-LASER SPECTROSCOPY; SELF-CONSISTENT-FIELD; BIOMOLECULAR BUILDING-BLOCKS; GAS-PHASE; HELIUM NANODROPLETS; IR-SPECTRA; AMINO-ACIDS; PHOTODISSOCIATION SPECTROSCOPY; SEMIEMPIRICAL POTENTIALS; BIOLOGICAL MOLECULES AB The results of anharmonic frequency calculations on neutral imidazole (C3N2H4, Im), protonated imidazole (ImH(+)), and its complexes with water (ImH(+))(H2O)(n), are presented and compared to gas phase infrared photodissociation spectroscopy (IRPD) data. Anharmonic frequencies are obtained via ab initio vibrational self-consistent field (VSCF) calculations taking into account pairwise interactions between the normal modes. The key results are: (1) Prediction of anharmonic vibrational frequencies on an MP2 ab initio potential energy surface show excellent agreement with experiment and outstanding improvement over the harmonic frequencies. For example, the ab initio calculated anharmonic frequency for (ImH(+))(H2O)N-2 exhibits an overall average percentage error of 0.6% from experiment. (2) Anharmonic vibrational frequencies calculated on a semiempirical potential energy surface fitted to ab initio harmonic data represents spectroscopy well, particularly for water complexes. As an example, anharmonic frequencies for (ImH(+))H2O and (ImH(+))(H2O)(2) show an overall average deviation of 1.02% and 1.05% from experiment, respectively. This agreement between theory and experiment also supports the validity and use of the pairwise approximation used in the calculations. (3) Anharmonic coupling due to hydration effects is found to significantly reduce the vibrational frequencies for the NH stretch modes. The frequency of the NH stretch is observed to increase with the removal of a water molecule or replacement of water with N-2. This result also indicates the ability of the VSCF method to predict accurate frequencies in a matrix environment. The calculation provides insights into the nature of anharmonic effects in the potential surface. Analysis of percentage anharmoncity in neutral Im and ImH(+) shows a higher percentage anharmonicity in the NH and CH stretch modes of neutral Im. Also, we observe that anharmonicity in the NH stretch modes of ImH(+) have some contribution from coupling effects, while that of neutral Im has no contribution whatsoever from mode-mode coupling. It is concluded that the incorporation of anharmonic effects in the calculation brings theory and experiment into much closer agreement for these systems. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. Tech Univ Berlin, Inst Opt & Atomare Phys, D-10623 Berlin, Germany. Hebrew Univ Jerusalem, Dept Phys Chem, IL-91904 Jerusalem, Israel. Hebrew Univ Jerusalem, Fritz Haber Res Ctr, IL-91904 Jerusalem, Israel. RP Gerber, RB (reprint author), NASA, Ames Res Ctr, Mail Stop T27B-1, Moffett Field, CA 94035 USA. EM benny@fh.huji.ac.il NR 53 TC 22 Z9 22 U1 0 U2 14 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD AUG 9 PY 2007 VL 111 IS 31 BP 7374 EP 7381 DI 10.1021/jp070785w PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 196JX UT WOS:000248478700016 PM 17500546 ER PT J AU Moore, TE Horwitz, JL AF Moore, T. E. Horwitz, J. L. TI Stellar ablation of planetary atmospheres SO REVIEWS OF GEOPHYSICS LA English DT Review ID SOLAR-WIND INTERACTION; SOFT-ELECTRON-PRECIPITATION; CLEFT ION FOUNTAIN; INTERPLANETARY MAGNETIC-FIELD; PLASMA SOURCE INSTRUMENT; IONOSPHERIC ACCELERATION MECHANISM; MASS-SPECTROMETER OBSERVATIONS; SPACECRAFT POTENTIAL CONTROL; HIGH-LATITUDE IONOSPHERE; RING CURRENT FORMATION AB We review observations and theories of the solar ablation of planetary atmospheres, focusing on the terrestrial case where a large magnetosphere holds off the solar wind, so that there is little direct atmospheric impact, but also couples the solar wind electromagnetically to the auroral zones. We consider the photothermal escape flows known as the polar wind or refilling flows, the enhanced mass flux escape flows that result from localized solar wind energy dissipation in the auroral zones, and the resultant enhanced neutral atom escape flows. We term these latter two escape flows the "auroral wind.'' We review observations and theories of the heating and acceleration of auroral winds, including energy inputs from precipitating particles, electromagnetic energy flux at magnetohydrodynamic and plasma wave frequencies, and acceleration by parallel electric fields and by convection pickup processes also known as `` centrifugal acceleration.'' We consider also the global circulation of ionospheric plasmas within the magnetosphere, their participation in magnetospheric disturbances as absorbers of momentum and energy, and their ultimate loss from the magnetosphere into the downstream solar wind, loading reconnection processes that occur at high altitudes near the magnetospheric boundaries. We consider the role of planetary magnetization and the accumulating evidence of stellar ablation of extrasolar planetary atmospheres. Finally, we suggest and discuss future needs for both the theory and observation of the planetary ionospheres and their role in solar wind interactions, to achieve the generality required for a predictive science of the coupling of stellar and planetary atmospheres over the full range of possible conditions. C1 NASA, Goddard Space Flight Ctr, Heliospher Phys Branch, Greenbelt, MD 20771 USA. Univ Texas, Dept Phys, Arlington, TX 76019 USA. RP Moore, TE (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Phys Branch, Code 612-2, Greenbelt, MD 20771 USA. EM tmoore@pop600.gsfc.nasa.gov; horwitz@uta.edu RI Moore, Thomas/D-4675-2012 OI Moore, Thomas/0000-0002-3150-1137 NR 258 TC 46 Z9 47 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 8755-1209 EI 1944-9208 J9 REV GEOPHYS JI Rev. Geophys. PD AUG 9 PY 2007 VL 45 IS 2 AR RG3002 DI 10.1029/2005RG000194 PG 34 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 202BQ UT WOS:000248876900001 ER PT J AU Futyan, JM Del Genio, AD AF Futyan, Joanna M. Del Genio, Anthony D. TI Relationships between lightning and properties of convective cloud clusters SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GLOBAL DISTRIBUTION; PART I; RADAR; PARAMETERIZATION; THUNDERSTORMS; DISTRIBUTIONS; CLIMATE AB Satellite observations of convective system properties and lightning flash rate are used to investigate the ability of potential lightning parameterizations to capture both the dominant land-ocean contrast in lightning occurrence and regional differences between Africa, the Amazon and the islands of the maritime continent. As found in previous studies, the radar storm height is tightly correlated with the lightning flash rate. A roughly second order power-law fit to the mean radar echo top height above the 0 degrees C isotherm is shown to capture both regional and land-ocean contrasts in lightning occurrence and flash rate using a single set of parameters. Recent developments should soon make it possible to implement a parameterization of this kind in global models. Parameterizations based on cloud top height, convective rain rate and convective rain fraction all require the use of separate fits over land and ocean and fail to capture observed differences between continental regions. C1 Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Futyan, JM (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. EM adelgenio@giss.nasa.gov RI Del Genio, Anthony/D-4663-2012 OI Del Genio, Anthony/0000-0001-7450-1359 NR 29 TC 17 Z9 17 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 8 PY 2007 VL 34 IS 15 AR L15705 DI 10.1029/2007GL030227 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 201ZQ UT WOS:000248871600002 ER PT J AU Ewing, SA Michalski, G Thiemens, M Quinn, RC Macalady, JL Kohl, S Wankel, SD Kendall, C Mckay, CP Amundson, R AF Ewing, Stephanie A. Michalski, Greg Thiemens, Mark Quinn, Richard C. Macalady, Jennifer L. Kohl, Steven Wankel, Scott D. Kendall, Carol Mckay, Christopher P. Amundson, Ronald TI Rainfall limit of the N cycle on Earth SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID ORGANIC NITROGEN DEPOSITION; OXYGEN ISOTOPIC COMPOSITION; ATACAMA DESERT; GLOBAL PATTERNS; MICROBIAL LIFE; ALKYL NITRATES; PACIFIC-OCEAN; FRESH-WATER; SOIL; CHILE AB In most climates on Earth, biological processes control soil N. In the Atacama Desert of Chile, aridity severely limits biology, and soils accumulate atmospheric NO3-. We examined this apparent transformation of the soil N cycle using a series of ancient Atacama Desert soils (> 2 My) that vary in rainfall (21 to < 2 mm yr(-1)). With decreasing rainfall, soil organic C decreases to 0.3 kg C m(-2) and biological activity becomes minimal, while soil NO3- and organic N increase to 4 kg N m(-2) and 1.4 kg N m(-2), respectively. Atmospheric NO3- (Delta O-17 = 23.0 parts per thousand) increases from 39% to 80% of total soil NO3- as rainfall decreases. These soils capture the transition from a steady state, biologically mediated soil N cycle to a dominantly abiotic, transient state of slowly accumulating atmospheric N. This transition suggests that oxidized soil N may be present in an even more arid and abiotic environment: Mars. C1 Univ Calif Berkeley, Dept Environm Sci Policy & Management, Div Ecosyst Sci, Berkeley, CA 94720 USA. USGS, Menlo Pk, CA 94025 USA. Desert Res Inst, Div Atmospher Sci, Reno, NV 89512 USA. Penn State Univ, Dept Geosci, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. Univ Calif San Diego, Div Phys Sci, La Jolla, CA 92093 USA. RP Ewing, SA (reprint author), Univ Calif Berkeley, Ctr Isotope Geochem, Dept Earth & Planetary Sci, 4767, Berkeley, CA 94720 USA. EM saewing@nature.berkeley.edu; gmichals@purdue.edu; mthiemens@ucsd.edu; rquinn@mail.arc.nasa.gov; jmacalad@geosc.psu.edu; steve.kohl@dri.edu; swankel@oeb.harvard.edu; ckendall@usgs.gov; cmckay@mail.arc.nasa.gov; earthy@nature.berkeley.edu RI Amundson, Ronald /E-2654-2015 NR 56 TC 27 Z9 27 U1 1 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD AUG 8 PY 2007 VL 21 IS 3 AR GB3009 DI 10.1029/2006GB002838 PG 12 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 201ZX UT WOS:000248872300002 ER PT J AU Rinsland, CP Dufour, G Boone, CD Bernath, PF Chiou, L Coheur, PF Turquety, S Clerbaux, C AF Rinsland, Curtis P. Dufour, Gaelle Boone, Chris D. Bernath, Peter F. Chiou, Linda Coheur, Pierre-Francois Turquety, Solene Clerbaux, Cathy TI Satellite boreal measurements over Alaska and Canada during June-July 2004: Simultaneous measurements of upper tropospheric CO, C2H6, HCN, CH3Cl, CH4, C2H2, CH3OH, HCOOH, OCS, and SF6 mixing ratios SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID TRANSFORM INFRARED-SPECTROSCOPY; BIOMASS-BURNING EMISSIONS; FOREST-FIRES; TRACE GASES; STRATOSPHERIC AEROSOL; ORGANIC-COMPOUNDS; CLIMATE-CHANGE; SAVANNA FIRES; ART.; CARBON AB Simultaneous ACE ( Atmospheric Chemistry Experiment) upper tropospheric CO, C2H6, HCN, CH3Cl, CH4, C2H2, CH3OH, HCOOH, and OCS measurements show plumes up to 185 ppbv (10(-9) per unit volume) for CO, 1.36 ppbv for C2H6, 755 pptv (10(-12) per unit volume) for HCN, 1.12 ppbv for CH3Cl, 1.82 ppmv (10(-6) per unit volume) for CH4, 0.178 ppbv for C2H2, 3.89 ppbv for CH3OH, 0.843 ppbv for HCOOH, and 0.48 ppbv for OCS in western Canada and Alaska at 50 degrees N-68 degrees N latitude between 29 June and 23 July 2004. Enhancement ratios and emission factors for HCOOH, CH3OH, HCN, C2H6, and OCS relative to CO at 250-350 hPa are inferred from measurements of young plumes compared with lower mixing ratios assumed to represent background conditions based on a CO emission factor derived from boreal measurements. Results are generally consistent with the limited data reported for various vegetative types and emission phases measured in extratropical forests including boreal forests. The low correlation between fire product emission mixing ratios and the SF6 mixing ratio is consistent with no significant SF6 emissions from the biomass fires. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. Sci Syst & Appl Inc, Hampton, VA 23666 USA. Univ Libre Bruxelles, B-1050 Brussels, Belgium. Univ Paris 06, Inst Pierre Simon Laplace, Serv Aeron, F-75252 Paris 05, France. Inst Pierre Simon Laplace, Meteorol Dynam Lab, F-91128 Palaiseau, France. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 401A, Hampton, VA 23681 USA. EM gaelle.dufour@lmd.polytechnique.fr; cboone@acebox.uwaterloo.ca; pfb500@york.ac.uk; l.s.chiou@larc.nasa.gov; pfcoheur@ulb.ac.be; stu@aero.jussieu.fr; ccl@aero.jussieu.fr RI Bernath, Peter/B-6567-2012; clerbaux, cathy/I-5478-2013 OI Bernath, Peter/0000-0002-1255-396X; NR 86 TC 45 Z9 45 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD AUG 8 PY 2007 VL 21 IS 3 AR GB3008 DI 10.1029/2006GB002795 PG 13 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 201ZX UT WOS:000248872300001 ER PT J AU Petukhov, AG Niggemann, J Smelyanskiy, VN Osipov, VV AF Petukhov, A. G. Niggemann, J. Smelyanskiy, V. N. Osipov, V. V. TI 100% spin accumulation in non-half-metallic ferromagnet-semiconductor junctions SO JOURNAL OF PHYSICS-CONDENSED MATTER LA English DT Article ID FIELD-EFFECT TRANSISTOR; QUANTUM-WELLS; INJECTION; INTERFACE; TRANSPORT; ELECTRON; VALVE; CONDUCTANCE; BARRIER; SPINTRONICS AB We show that the spin polarization of electron density in non-magnetic degenerate semiconductors can achieve 100%. The effect of 100% spin accumulation does not require a half-metallic ferromagnetic contact and can be realized in ferromagnet-semiconductor FM-n(+)-n junctions even at moderate spin selectivity of the FM-n(+) contact when the electrons with spin 'up' are extracted from n semiconductor through the heavily doped n(+) layer into the ferromagnet and the electrons with spin 'down' are accumulated near the n(+)-n interface. We derived a general equation relating spin polarization of the current to that of the electron density in non-magnetic semiconductors. We found that the effect of complete spin polarization is achieved near the n(+)-n interface when the concentration of the spin 'up' electrons tends to zero in this region while the diffusion current of these electrons remains finite. C1 S Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Mission Crit Technol Inc, El Segundo, CA 90245 USA. RP Petukhov, AG (reprint author), S Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. NR 78 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-8984 EI 1361-648X J9 J PHYS-CONDENS MAT JI J. Phys.-Condes. Matter PD AUG 8 PY 2007 VL 19 IS 31 AR 315205 DI 10.1088/0953-8984/19/31/315205 PG 16 WC Physics, Condensed Matter SC Physics GA 192FH UT WOS:000248185700006 PM 21694106 ER PT J AU Androulakis, J Lin, CH Kong, HJ Uher, C Wu, CI Hogan, T Cook, BA Caillat, T Paraskevopoulos, KM Kanatzidis, MG AF Androulakis, John Lin, Chia-Her Kong, Hun-Jin Uher, Ctirad Wu, Chun-I Hogan, Timothy Cook, Bruce A. Caillat, Thierry Paraskevopoulos, Konstantinos M. Kanatzidis, Mercouri G. TI Spinodal decomposition and nucleation and growth as a means to bulk nanostructured thermoelectrics: Enhanced performance in Pb1-xSnxTe-PbS SO JOURNAL OF THE AMERICAN CHEMICAL SOCIETY LA English DT Article ID QUANTUM-DOT SUPERLATTICE; OFF-CENTER IMPURITIES; SYSTEM PBS-PBTE; THERMAL-CONDUCTIVITY; SOLID-SOLUTIONS; MERIT ENHANCEMENT; ROOM-TEMPERATURE; POLYMER BLENDS; FIGURE; ALLOYS AB The solid-state transformation phenomena of spinodal decomposition and nucleation and growth are presented as tools to create nanostructured thermoelectric materials with very low thermal conductivity and greatly enhanced figure of merit. The systems (PbTe)(1-x)(PbS)(x) and (Pb0.95Sn0.05Te)(1-x)(PbS)(x) are not solid solutions but phase separate into PbTe-rich and PbS-rich regions to produce coherent nanoscale heterogeneities that severely depress the lattice thermal conductivity. For x > similar to 0.03 the materials are ordered on three submicrometer length scales. Transmission electron microscopy reveals both spinodal decomposition and nucleation and growth phenomena the relative magnitude of which varies with x. We show that the (Pb0.95Sn0.05Te)(1-x)(PbS)(x) system, despite its nanostructured nature, maintains a high electron mobility (> 100 cm(2)/V center dot s at 700 K). At x similar to 0.08 the material achieves a very low room-temperature lattice thermal conductivity of similar to 0.4 W/m center dot K. This value is only 28% of the PbTe lattice thermal conductivity at room temperature. The inhibition of heat flow in this system is caused by nanostructure-induced acoustic impedance mismatch between the PbTe-rich and PbS-rich regions. As a result the thermoelectric properties of (Pb0.95Sn0.05Te)(1-x)(PbS)(x) at x = 0.04, 0.08, and 0.16 were found to be superior to those of PbTe by almost a factor of 2. The relative importance of the two observed modes of nanostructuring, spinodal decomposition and nucleation and growth, in suppressing the thermal conductivity was assessed in this work, and we can conclude that the latter mode seems more effective in doing so. The promise of such a system for high efficiency is highlighted by a ZT similar to 1.50 at 642 K for x similar to 0.08. C1 Michigan State Univ, Dept Chem, E Lansing, MI 48824 USA. Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. Iowa State Univ, Ames Lab, Mat & Engn Phys Program, Ames, IA 50011 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Aristotle Univ Thessaloniki, Dept Phys, Thessaloniki 54124, Greece. Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. RP Kanatzidis, MG (reprint author), Michigan State Univ, Dept Chem, E Lansing, MI 48824 USA. EM m-kanatzidis@northwestern.edu RI Paraskeuopoulos, Konstantinos/F-9926-2011; Lin, Chia-Her/L-7009-2014 OI Lin, Chia-Her/0000-0002-1360-0828 NR 57 TC 270 Z9 272 U1 30 U2 163 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0002-7863 J9 J AM CHEM SOC JI J. Am. Chem. Soc. PD AUG 8 PY 2007 VL 129 IS 31 BP 9780 EP 9788 DI 10.1021/ja071875h PG 9 WC Chemistry, Multidisciplinary SC Chemistry GA 196LW UT WOS:000248484400060 PM 17629270 ER PT J AU Stager, JC Ruzmaikin, A Conway, D Verburg, P Mason, PJ AF Stager, J. Curt Ruzmaikin, Alexander Conway, Declan Verburg, Piet Mason, Peter J. TI Sunspots, El Nino, and the levels of Lake Victoria, East Africa SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NORTH-ATLANTIC CLIMATE; SOLAR INFLUENCE; INDIAN-OCEAN; WATER-BALANCE; ASIAN MONSOON; LAST MILLENNIUM; COSMIC-RAYS; ARABIAN SEA; SHORT RAINS; NILE BASIN AB An association of high sunspot numbers with rises in the level of Lake Victoria, East Africa, has been the focus of many investigations and vigorous debate during the last century. In this paper, we show that peaks in the similar to 11- year sunspot cycle were accompanied by Victoria level maxima throughout the 20th century, due to the occurrence of positive rainfall anomalies similar to 1 year before solar maxima. Similar patterns also occurred in at least five other East African lakes, which indicates that these sunspot-rainfall relationships were broadly regional in scale. Although irradiance fluctuations associated with the sunspot cycle are weak, their effects on tropical rainfall could be amplified through interactions with sea surface temperatures and atmospheric circulation systems, including ENSO. If this Sun-rainfall relationship persists in the future, then sunspot cycles can be used for long-term prediction of precipitation anomalies and associated outbreaks of insect-borne disease in much of East Africa. In that case, unusually wet rainy seasons and Rift Valley Fever epidemics should occur a year or so before the next solar maximum, which is expected to occur in 2011-2012 AD. C1 Paul Smiths Coll, Div Nat Sci, Paul Smiths, NY 12970 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Maine, Climate Change Inst, Orono, ME USA. Univ E Anglia, Sch Dev Studies, Norwich NR4 7TJ, Norfolk, England. Univ Georgia, Inst Ecol, Athens, GA 30602 USA. MWH UK Ltd, Int Dams & Hydropower, High Wycombe HP13 5AJ, Bucks, England. RP Stager, JC (reprint author), Paul Smiths Coll, Div Nat Sci, Paul Smiths, NY 12970 USA. EM cstager@paulsmiths.edu; alexander.ruzmaikin@jpl.nasa.gov; d.conway@uea.ac.uk; verburg@uga.edu; peter.j.mason@mwhglobal.com OI verburg, piet/0000-0001-7574-9161 NR 95 TC 26 Z9 26 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 7 PY 2007 VL 112 IS D15 AR D15106 DI 10.1029/2006JD008362 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 202AA UT WOS:000248872600008 ER PT J AU Aksak, B Sitti, M Cassell, A Li, J Meyyappan, M Callen, P AF Aksak, Burak Sitti, Metin Cassell, Alan Li, Jun Meyyappan, Meyya Callen, Phillip TI Friction of partially embedded vertically aligned carbon nanofibers inside elastomers SO APPLIED PHYSICS LETTERS LA English DT Article ID SURFACES; GROWTH; ARRAYS AB Vertically aligned carbon nanofibers partially embedded inside polyurethane (eVACNFs) are proposed as a robust high friction fibrillar material with a compliant backing. Carbon nanofibers with 50-150 nm in diameter and 20-30 mu m in length are vertically grown on silicon and transferred completely inside an elastomer by vacuum molding. By using time controlled and selective oxygen plasma etching, fibers are partially released up to 5 mu m length. Macroscale friction experiments show that eVACNFs exhibit reproducible effective friction coefficients up to 1. Besides high friction, the proposed fabrication method improves fiber-substrate bond strength, and enables uniform height nanofibers with a compliant backing. C1 Carnegie Mellon Univ, Dept Mech Engn, NanoRobot Lab, Pittsburgh, PA 15213 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Sitti, M (reprint author), Carnegie Mellon Univ, Dept Mech Engn, NanoRobot Lab, Pittsburgh, PA 15213 USA. EM sitti@cmu.edu RI Li, Jun/H-7771-2013 OI Li, Jun/0000-0002-3689-8946 NR 12 TC 31 Z9 32 U1 1 U2 18 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 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD AUG 6 PY 2007 VL 91 IS 6 AR 061906 DI 10.1063/1.2767997 PG 3 WC Physics, Applied SC Physics GA 198XS UT WOS:000248661400033 ER PT J AU Raissi, H Moshfeghi, E Jalbout, AF Hossein, MS Fazli, M AF Raissi, Heidar Moshfeghi, Effat Jalbout, Abraham F. Hossein, Mohammad Saeid Fazli, Mustapha TI An approach to estimate the energy and strength of the intramolecular hydrogen bond in different conformers of 4-methylamino-3-penten-2-one SO INTERNATIONAL JOURNAL OF QUANTUM CHEMISTRY LA English DT Article DE 4-methylamino-3-penten-2-one; intramolecular hydrogen bond; alpha,beta-unsaturated-beta-ketoenamines; related rotamers method; ab initio; AIM calculations ID VIBRATIONAL ASSIGNMENT; CHARGE-DENSITY; AB-INITIO; MOLECULES; ATOMS AB The molecular structure and intramolecular hydrogen bond energy of 32 conformers of 4-methylamino-3-penten-2-one were investigated at MP2 and B3LYP levels of theory using the standard 6-31G** basis set and AIM analyses. Furthermore, calculations for all the possible conformations of 4-methylamino-3-penten-2-one in water solution were also carried out at B3LYP/6-31G** level of theory. The calculated geometrical parameters and conformational analyses in gas phase and water solution show that the ketoamine conformers of this compound are more stable than the other conformers (i.e., enolimine and ketoimine). This stability is mainly due to the formation of a strong N-H center dot center dot center dot O intramolecular hydrogen bond, which is assisted by pi-electrons resonance. Hydrogen bond energies for all conformers of 4-methylamino-3-penten-2-one were obtained from the related rotamers method. The nature of intramolecular hydrogen bond existing within 4-methylamino-3-penten-2-one has been investigated by means of the Bader theory of atoms in molecules, which is based on topological properties of the electron density. The results of these calculations support the results which obtained by related rotamers method. (c) 2007 Wiley Periodicals, Inc. C1 Birjand Univ, Dept Chem, Birjand, Iran. Univ Nacl Autonoma Mexico, Inst Chem, Mexico City 04510, DF, Mexico. Univ Arizona, Dept Chem, NASA, Astrobiol Inst, Tucson, AZ 85721 USA. Semnan Univ, Dept Chem, Semnan, Iran. RP Moshfeghi, E (reprint author), Birjand Univ, Dept Chem, Birjand, Iran. EM e.moshfeghi@yahoo.com NR 19 TC 13 Z9 13 U1 1 U2 4 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0020-7608 J9 INT J QUANTUM CHEM JI Int. J. Quantum Chem. PD AUG 5 PY 2007 VL 107 IS 9 BP 1835 EP 1845 DI 10.1002/qua.21310 PG 11 WC Chemistry, Physical; Mathematics, Interdisciplinary Applications; Physics, Atomic, Molecular & Chemical SC Chemistry; Mathematics; Physics GA 164QI UT WOS:000246248400001 ER PT J AU Liu, Y de Jeu, RAM van Dijk, AIJM Owe, M AF Liu, Yi de Jeu, Richard A. M. van Dijk, Albert I. J. M. Owe, Manfred TI TRMM-TMI satellite observed soil moisture and vegetation density (1998-2005) show strong connection with El Nino in eastern Australia SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID POLARIZATION DIFFERENCE INDEX; OPTICAL DEPTH RETRIEVAL; SEA-SURFACE TEMPERATURE; SOUTHERN OSCILLATION; MICROWAVE EMISSION; INDIAN-OCEAN; RAINFALL; METHODOLOGY; VARIABILITY; CIRCULATION AB Spatiotemporal patterns in soil moisture and vegetation water content across mainland Australia were investigated from 1998 through 2005, using TRMM/TMI passive microwave observations. The Empirical Orthogonal Function technique was used to extract dominant spatial and temporal patterns in retrieved estimates of moisture content for the top 1-cm of soil (theta) and vegetation moisture content (via optical depth tau). The dominant temporal theta and tau patterns were strongly correlated to the El Nino Southern Oscillation Index (SOI) in spring (r(2) = 0.90), and to a progressively lesser extent autumn, summer and winter. The Indian Ocean Dipole (IOD) index also explained part of the variation in spring theta and tau. Correlation analysis suggested that the regions most affected by El Nino are mainly located in eastern Australia. The results suggest that the drought conditions experienced in eastern Australia since 2000 and clearly expressed in these satellite observations have a strong connection with El Nino. C1 Vrije Univ Amsterdam, Fac Earth & Life Sci, Dept Hydrol & Geoenvironm Sci, NL-1081 HV Amsterdam, Netherlands. CSIRO, Div Land & Water, Black Mt Lab, Canberra, ACT 2601, Australia. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Liu, Y (reprint author), Vrije Univ Amsterdam, Fac Earth & Life Sci, Dept Hydrol & Geoenvironm Sci, NL-1081 HV Amsterdam, Netherlands. RI Van Dijk, Albert/B-3106-2011; Liu, Yi/H-9226-2013; Liu, Yi/M-7169-2015 OI Van Dijk, Albert/0000-0002-6508-7480; Liu, Yi/0000-0001-9059-8269 NR 30 TC 25 Z9 25 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 4 PY 2007 VL 34 IS 15 AR L15401 DI 10.1029/2007GL030311 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 198AK UT WOS:000248599200001 ER PT J AU Niu, GY Seo, KW Yang, ZL Wilson, C Su, H Chen, J Rodell, M AF Niu, Guo-Yue Seo, Ki-Weon Yang, Zong-Liang Wilson, Clark Su, Hua Chen, Jianli Rodell, Matthew TI Retrieving snow mass from GRACE terrestrial water storage change with a land surface model SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VARIABILITY; EQUIVALENT; UNCERTAINTY; SYSTEM; SOIL AB A reliable snow water equivalent (SWE) product is critical for climate and hydrology studies in Arctic regions. Passive microwave sensors aboard satellites provide a capability of observing global SWE and have produced many SWE datasets. However, these datasets have significant errors in boreal forest regions and where snowpack is deep or wet. The Gravity Recovery and Climate Experiment (GRACE) satellites are measuring changes in terrestrial water storage (TWS), of which snow mass is the primary component in winter Arctic river basins. This paper shows SWE can be derived from GRACE TWS change in regions where the ground is not covered by snow in a summer month if accurate changes in below-ground water storage (including soil water and groundwater) can be provided by a land surface model. Based on gravity change, the GRACE-derived SWE estimates are not affected by the boreal forest canopy and are more accurate in deep snow regions than microwave retrievals. The paper also discusses the uncertainties in the SWE retrievals. C1 Univ Texas, John A & Katherine G Jackson Sch Geosci, Dept Geol, Austin, TX 78712 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Niu, GY (reprint author), Univ Texas, John A & Katherine G Jackson Sch Geosci, Dept Geol, Austin, TX 78712 USA. RI Yang, Zong-Liang/B-4916-2011; Rodell, Matthew/E-4946-2012; Niu, Guo-Yue/B-8317-2011 OI Rodell, Matthew/0000-0003-0106-7437; NR 23 TC 27 Z9 29 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 4 PY 2007 VL 34 IS 15 AR L15704 DI 10.1029/2007GL030413 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 198AK UT WOS:000248599200002 ER PT J AU Paranicas, C Mauk, BH Khurana, K Jun, I Garrett, H Krupp, N Roussos, E AF Paranicas, C. Mauk, B. H. Khurana, K. Jun, I. Garrett, H. Krupp, N. Roussos, E. TI Europa's near-surface radiation environment SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GALILEO SPACECRAFT; MAGNETOSPHERE; DISTRIBUTIONS; PARTICLES AB As flux tubes are carried over Europa, hundreds of keV to tens of MeV electrons are absorbed by the moon due to their short bounce times. This results in an asymmetry in energetic charged particles in the near surface environment and in the bombardment of Europa's surface. For example, electrons between about 0.1 and 50 MeV do not have direct access to more than 50% of the sphere at 100 km Europa altitude. Moreover, a hypothetical orbiting spacecraft at this altitude would see a reduction of about 33% of the sky, based on Europa's obstructing its field-of-view. We find that the predicted radiation reduction due to the moon's presence is consistent with data from Galileo's Energetic Particles Detector (EPD). In this paper, we present data that illustrate this consistency and use standard models of the radiation environment to evaluate the energetic electron fluence at 100 km. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Max Planck Inst Sonnensystemforsch, D-37191 Katlenburg Duhm, Germany. RP Paranicas, C (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. RI Roussos, Elias/H-2249-2011; Paranicas, Christopher/B-1470-2016; Mauk, Barry/E-8420-2017; OI Paranicas, Christopher/0000-0002-4391-8255; Mauk, Barry/0000-0001-9789-3797; Roussos, Elias/0000-0002-5699-0678 NR 14 TC 11 Z9 11 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 4 PY 2007 VL 34 IS 15 AR L15103 DI 10.1029/2007GL030834 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 198AK UT WOS:000248599200005 ER PT J AU Leask, HJ Wilson, L Mitchell, KL AF Leask, Harald J. Wilson, Lionel Mitchell, Karl L. TI Formation of Mangala Valles outflow channel, Mars: Morphological development and water discharge and duration estimates SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SIZE-FREQUENCY DISTRIBUTIONS; CERBERUS FOSSAE; SEDIMENT TRANSPORT; SAPPING PROCESSES; MARTIAN CHANNELS; ATHABASCA-VALLES; GROUNDWATER; ICE; FLOODS; FLOWS AB The morphology of features on the floor of the Mangala Valles suggests that the channel system was not bank-full for most of the duration of its formation by water being released from its source, the Mangala Fossa graben. For an estimated typical 50 m water depth, local slopes of sin alpha = similar to 0.002 imply a discharge of similar to 1 x 10(7) m(3) s(-1), a water flow speed of similar to 9 m s(-1), and a subcritical Froude number of similar to 0.7-0.8. For a range of published estimates of the volume of material eroded from the channel system this implies a duration of similar to 17 days if the sediment carrying capacity of the similar to 15,000 km(3) of water involved had been 40% by volume. If the sediment load had been 20% by volume, the duration would have been similar to 46 days and the water volume required would have been similar to 40,000 km(3). Implied bed erosion rates lie in the range similar to 1 to similar to 12 m/day. If the system had been bank-full during the early stages of channel development the discharge could have been up to similar to 10(8) m(3) s(-1), with flow speeds of similar to 15 m s(-1) and a subcritical Froude number of similar to 0.4-0.5. C1 Univ Lancaster, Inst Environm & Nat Sci, Dept Environm Sci, Planetary Sci Res Grp, Lancaster LA1 4YQ, England. Jet Propuls Lab, Pasadena, CA 91109 USA. RP Leask, HJ (reprint author), Univ Lancaster, Inst Environm & Nat Sci, Dept Environm Sci, Planetary Sci Res Grp, Lancaster LA1 4YQ, England. NR 63 TC 17 Z9 17 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 4 PY 2007 VL 112 IS E8 AR E08003 DI 10.1029/2006JE002851 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 198BT UT WOS:000248602700003 ER PT J AU Zhou, YP Kratz, DP Wilber, AC Gupta, SK Cess, RD AF Zhou, Yaping Kratz, David P. Wilber, Anne C. Gupta, Shashi K. Cess, Robert D. TI An improved algorithm for retrieving surface downwelling longwave radiation from satellite measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CLIMATE RESEARCH; SOLAR-RADIATION; CLOUD; NETWORK; CERES AB [1] Zhou and Cess (2001) developed an algorithm for retrieving surface downwelling longwave radiation (SDLW) based upon detailed studies using radiative transfer model calculations and surface radiometric measurements. The algorithm links clear sky SDLW with surface upwelling longwave (LW) flux and column precipitable water vapor. For cloudy sky cases, the cloud liquid water path is used as an additional parameter to account for the effects of clouds. Despite the simplicity of the algorithm, it performs very well for most geographical regions except for those regions where the atmospheric conditions near the surface tend to be extremely cold and dry. Systematic errors are also found for scenes that are covered with ice clouds. An improved version of the algorithm prevents the large errors in the SDLWat low water vapor amounts by taking into account that, under such conditions, the SDLW and water vapor amount are nearly linear in their relationship. The new algorithm also utilizes cloud fraction and cloud liquid and ice water paths available from the Cloud and the Earth's Radiant Energy System (CERES) single- scanner footprint (SSF) product to separately compute the clear and cloudy portions of the fluxes. The new algorithm has been validated against surface measurements at 29 stations around the globe for Terra and Aqua satellites. The results show significant improvement over the original version. Preliminary tests also suggest that the new algorithm works quite well for high elevation locations such as Tibet site where current satellite products exhibit large biases. The revised Zhou-Cess algorithm is also slightly better or comparable to more sophisticated algorithms currently implemented in the CERES processing and will be incorporated as one of the CERES empirical surface radiation algorithms. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol, Catonsville, MD 21228 USA. NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA. Analyt Serv & Mat Inc, Hampton, VA 23666 USA. SUNY Stony Brook, Marine Sci Res Ctr, Stony Brook, NY 11794 USA. RP Zhou, YP (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol, Catonsville, MD 21228 USA. EM yaping.zhou.1@gsfc.nasa.gov RI wilber, anne/F-6270-2011 NR 26 TC 25 Z9 25 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 3 PY 2007 VL 112 IS D15 AR D15102 DI 10.1029/2006JD008159 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 198AU UT WOS:000248600200002 ER PT J AU Ramanathan, V Ramana, MV Roberts, G Kim, D Corrigan, C Chung, C Winker, D AF Ramanathan, Veerabhadran Ramana, Muvva V. Roberts, Gregory Kim, Dohyeong Corrigan, Craig Chung, Chul Winker, David TI Warming trends in Asia amplified by brown cloud solar absorption SO NATURE LA English DT Article ID CLIMATE-CHANGE; MODEL; IMPACTS; GLACIER AB Atmospheric brown clouds are mostly the result of biomass burning and fossil fuel consumption(1). They consist of a mixture of light-absorbing and light-scattering aerosols(1) and therefore contribute to atmospheric solar heating and surface cooling. The sum of the two climate forcing terms-the net aerosol forcing effect is thought to be negative and may have masked as much as half of the global warming attributed to the recent rapid rise in greenhouse gases(2). There is, however, at least a fourfold uncertainty(2) in the aerosol forcing effect. Atmospheric solar heating is a significant source of the uncertainty, because current estimates are largely derived from model studies. Here we use three lightweight unmanned aerial vehicles that were vertically stacked between 0.5 and 3 km over the polluted Indian Ocean. These unmanned aerial vehicles deployed miniaturized instruments measuring aerosol concentrations, soot amount and solar fluxes. During 18 flight missions the three unmanned aerial vehicles were flown with a horizontal separation of tens of metres or less and a temporal separation of less than ten seconds, which made it possible to measure the atmospheric solar heating rates directly. We found that atmospheric brown clouds enhanced lower atmospheric solar heating by about 50 per cent. Our general circulation model simulations, which take into account the recently observed widespread occurrence of vertically extended atmospheric brown clouds over the Indian Ocean and Asia(3), suggest that atmospheric brown clouds contribute as much as the recent increase in anthropogenic greenhouse gases to regional lower atmospheric warming trends. We propose that the combined warming trend of 0.25 K per decade may be sufficient to account for the observed retreat of the Himalayan glaciers(4-6). C1 Univ Calif San Diego, Scripps Inst Oceanog, Ctr Clouds Chem & Climate, La Jolla, CA 92037 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Ramanathan, V (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Clouds Chem & Climate, La Jolla, CA 92037 USA. EM vramanathan@ucsd.edu NR 25 TC 363 Z9 380 U1 17 U2 112 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 2 PY 2007 VL 448 IS 7153 BP 575 EP U5 DI 10.1038/nature06019 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 195XV UT WOS:000248446700039 PM 17671499 ER PT J AU Sherwood, B AF Sherwood, Brent TI Untitled SO AEROSPACE AMERICA LA English DT Letter C1 NASA, Jet Propuls Lab, Pasadena, CA USA. RP Sherwood, B (reprint author), NASA, Jet Propuls Lab, Pasadena, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0740-722X J9 AEROSPACE AM JI Aerosp. Am. PD AUG PY 2007 VL 45 IS 8 BP 7 EP 7 PG 1 WC Engineering, Aerospace SC Engineering GA 196ZA UT WOS:000248521000006 ER PT J AU Beresh, SJ Heineck, JT Walker, SM Schairer, ET Yaste, DM AF Beresh, Steven J. Heineck, James T. Walker, Stephen M. Schairer, Edward T. Yaste, David M. TI Planar velocimetry of jet/fin interaction on a full-scale flight vehicle configuration SO AIAA JOURNAL LA English DT Article ID TRANSVERSE SUPERSONIC JET; PARTICLE IMAGE VELOCIMETRY; COMPRESSIBLE CROSS-FLOW AB Stereoscopic particle image velocimetry has been implemented in a production-scale transonic wind tunnel for studying jet/fin interaction created by exhaust plumes from spin rockets on a full-scale model of a finned body of revolution. Data acquired just upstream of the leading edge of the fin root clearly display the counter-rotating vortex pair that dominates the interaction far field and the remnant of the horseshoe vortex near the vehicle surface. The counter-rotating vortex pair is distinctly asymmetric due to originating from a scarfed nozzle and displays some rotation with respect to the model surface. Velocity fields measured over a range of flowfield conditions and model orientations show that the vortex of negative sign is always closer to the fins than its positive counterpart and does not greatly change location as flowfield parameters are altered. The circulation of this vortex correlates with a reduction in the simultaneously measured vehicle roll torque. Further correlations are hindered by untreatable bias errors in the velocimetry. Instead, a model of the vortex structure derived from the velocimetry data reveals that the angle of attack induced upon the fins by the counter-rotating vortex pair correlates with the roll torque loss. Similar correlations suggest that in level flight this effect is dominant, but at angle of attack the horseshoe vortex on the windward side has an additional influence. C1 Sandia Natl Labs, Engn Sci Ctr, Albuquerque, NM 87185 USA. NASA, Ames Res Ctr, Expt Aerophys Branch, Moffett Field, CA 94035 USA. RP Beresh, SJ (reprint author), Sandia Natl Labs, Engn Sci Ctr, POB 5800,Mailstop 0834, Albuquerque, NM 87185 USA. NR 21 TC 3 Z9 4 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD AUG PY 2007 VL 45 IS 8 BP 1827 EP 1840 DI 10.2514/1.26485 PG 14 WC Engineering, Aerospace SC Engineering GA 195BE UT WOS:000248386700005 ER PT J AU Khorrami, MR Choudhari, MM Lockard, DP Jenkins, LN McGinley, CB AF Khorrami, Mehdi R. Choudhari, Meelan M. Lockard, David P. Jenkins, Luther N. McGinley, Catherine B. TI Unsteady flowfield around tandem cylinders as prototype component interaction in airframe noise SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/CEAS 11th Aeroacoustics Conference CY MAY 23-25, 2005 CL Monterey, CA SP AIAA, CEAS ID 2 CIRCULAR-CYLINDERS; SUPERCRITICAL REYNOLDS-NUMBER; IN-LINE ARRANGEMENT; PRESSURE-FLUCTUATIONS; FLOW; INTERFERENCE; SURFACE; COMPUTATIONS; TURBULENCE; TUBES AB The current effort characterizes the details of flow interactions and wake interference effects between two cylinders in a tandem configuration. This setup is representative of several component-level How interactions that occur when air flows over the main landing gear of aircraft. Such interactions are likely to have a significant impact on the noise radiation associated with the undercarriage. This paper focuses on two-dimensional, time-accurate flow simulations of two distinct tandem cylinder flow regimes, associated with short and intermediate separation distances between the two cylinders. Unsteady Reynolds averaged Navier-Stokes simulations using a two-equation turbulence model run at a Reynolds number of 1.66 x 10(5) and a Mach number of 0.166 are presented. Emphasis is placed on understanding both the time-averaged and unsteady flow features between the two cylinders and in the wake of the rear cylinder. Predicted mean-flow quantities and vortex shedding frequencies show reasonable agreement with measured data for both cylinder spacings. Computations for the short separation distance exhibit a nonphysical decay of How unsteadiness with time; however, the predicted sensitivity of the mean lift coefficient to small variations in the upstream How angularity explains the asymmetric flowfield observed in the present and previous measurements. C1 NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA. RP Khorrami, MR (reprint author), NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 NR 29 TC 23 Z9 23 U1 0 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD AUG PY 2007 VL 45 IS 8 BP 1930 EP 1941 DI 10.2514/1.23690 PG 12 WC Engineering, Aerospace SC Engineering GA 195BE UT WOS:000248386700014 ER PT J AU Inger, GR Moss, JN AF Inger, George R. Moss, James N. TI Comparison of Navier-Stokes and direct simulation Monte Carlo predictions with separation SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 36th Fluid Dynamics Conference CY JUN 05-08, 2006 CL San Francisco, CA SP Amer Inst Aeronaut & Astronaut C1 NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. Iowa State Univ, Ames, IA 50011 USA. RP Inger, GR (reprint author), Iowa State Univ, 2271 Howe Hall,Room 1200, Ames, IA 50011 USA. EM inger@iastate.edu; j.n.moss@larc.nasa.gov NR 8 TC 1 Z9 1 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD AUG PY 2007 VL 45 IS 8 BP 2102 EP 2106 DI 10.2514/1.28278 PG 5 WC Engineering, Aerospace SC Engineering GA 195BE UT WOS:000248386700035 ER PT J AU Dillon, JG Fishbain, S Miller, SR Bebout, BM Habicht, KS Webb, SM Stahl, DA AF Dillon, Jesse G. Fishbain, Susan Miller, Scott R. Bebout, Brad M. Habicht, Kirsten S. Webb, Samuel M. Stahl, David A. TI High rates of sulfate reduction in a low-sulfate hot spring microbial mat are driven by a low level of diversity of sulfate-respiring microorganisms SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID SOLAR LAKE SINAI; ALGAL-BACTERIAL MAT; CYANOBACTERIAL MATS; REDUCING BACTERIA; SULFUR CYCLE; IN-SITU; SP-NOV; SEDIMENTS; RESPIRATION; COMMUNITY AB The importance of sulfate respiration in the microbial mat found in the low-sulfate thermal outflow of Mushroom Spring in Yellowstone National Park was evaluated using a combination of molecular, microelectrode, and radiotracer studies. Despite very low sulfate concentrations, this mat community was shown to sustain a highly active sulfur cycle. The highest rates of sulfate respiration were measured close to the surface of the mat late in the day when photosynthetic oxygen production ceased and were associated with a Thermodesuffiovibrio-like population. Reduced activity at greater depths was correlated with novel populations of sulfate-reducing microorganisms, unrelated to characterized species, and most likely due to both sulfate and carbon limitation. C1 Univ Washington, Dept Microbiol, Seattle, WA 98195 USA. Univ Washington, NASA, Astrobiol Inst, Seattle, WA 98195 USA. Northwestern Univ, Dept Civil & Environm Engn, Evanston, IL 60208 USA. Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 95035 USA. Univ So Denmark, Nord Ctr Earth Evolut, Odense, Denmark. Univ So Denmark, Inst Biol, Odense, Denmark. Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. RP Dillon, JG (reprint author), Calif State Univ Long Beach, Dept Biol Sci, Long Beach, CA 90840 USA. EM jdillon@csulb.edu RI Webb, Samuel/D-4778-2009 OI Webb, Samuel/0000-0003-1188-0464 NR 48 TC 23 Z9 23 U1 1 U2 16 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD AUG PY 2007 VL 73 IS 16 BP 5218 EP 5226 DI 10.1128/AEM.00357-07 PG 9 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 201IY UT WOS:000248825900019 PM 17575000 ER PT J AU Mueller, ER Henschke, R Robotham, WE Newman, LA Laughman, LM Hart, RA Kennedy, J Pickett, HM AF Mueller, Eric R. Henschke, Robert Robotham, William E., Jr. Newman, Leon A. Laughman, Lanny M. Hart, Richard A. Kennedy, John Pickett, Herbert M. TI Terahertz local oscillator for the microwave limb sounder on the aura satellite SO APPLIED OPTICS LA English DT Article ID OPTICALLY PUMPED LASER; 118 MU-M; LIGHT SHIFT; OPERATION AB The Microwave Limb Sounder on the Aura satellite has a radiometer at 2.5 THz to perform global mapping of OH in the atmosphere. The OH radiometer utilizes two Schottky-diode mixers pumped by an optically pumped THz gas laser local oscillator. The laser was first turned on in space on July 22, 2004, and has performed without issue for more than 30 months. The specifications, design, and modeling of this 2.5 THz laser local oscillator are presented here, along with some of the important design validation and test results. (c) 2007 Optical Society of America. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Coherent Inc, Bloomfield, CT 06002 USA. RP Pickett, HM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM herbert.m.pickett@jpl.nasa.gov NR 15 TC 15 Z9 19 U1 1 U2 1 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 AUG 1 PY 2007 VL 46 IS 22 BP 4907 EP 4915 DI 10.1364/AO.46.004907 PG 9 WC Optics SC Optics GA 206EQ UT WOS:000249167100008 PM 17676094 ER PT J AU Franz, BA Bailey, SW Werdell, PJ McClain, CR AF Franz, Bryan A. Bailey, Sean W. Werdell, P. Jeremy McClain, Charles R. TI Sensor-independent approach to the vicarious calibration of satellite ocean color radiometry SO APPLIED OPTICS LA English DT Article ID WATER-LEAVING RADIANCE; ATMOSPHERIC CORRECTION; SPECTRAL REFLECTANCE; SEAWIFS DATA; VALIDATION; INSTRUMENT; WHITECAPS; ALGORITHM; SURFACE AB The retrieval of ocean color radiometry from space-based sensors requires on-orbit vicarious calibration to achieve the level of accuracy desired for quantitative oceanographic applications. The approach developed by the NASA Ocean Biology Processing Group (OBPG) adjusts the integrated instrument and atmospheric correction system to retrieve normalized water-leaving radiances that are in agreement with ground truth measurements. The method is independent of the satellite sensor or the source of the ground truth data, but it is specific to the atmospheric correction algorithm. The OBPG vicarious calibration approach is described in detail, and results are presented for the operational calibration of SeaWiFS using data from the Marine Optical Buoy (MOBY) and observations of clear-water sites in the South Pacific and southern Indian Ocean. It is shown that the vicarious calibration allows SeaWiFS to reproduce the MOBY radiances and achieve good agreement with radiometric and chlorophyll a measurements from independent in situ sources. We also find that the derived vicarious gains show no significant temporal or geometric dependencies, and that the mission-average calibration reaches stability after -20-40 high-quality calibration samples. Finally, we demonstrate that the performance of the vicariously calibrated retrieval system is relatively insensitive to the assumptions inherent in our approach. (c) 2007 Optical Society of America. C1 NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA. Sci Applicat Int Corp, San Diego, CA 92121 USA. Futuretech Corp, Greenbelt, MD 20770 USA. Sci Syst & Appl Inc, Lanham, MD 20706 USA. RP Franz, BA (reprint author), NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, 614-8, Greenbelt, MD 20771 USA. EM bryan.franz@gsfc.nasa.gov RI Franz, Bryan/D-6284-2012; Werdell, Jeremy/D-8265-2012; Bailey, Sean/D-3077-2017 OI Franz, Bryan/0000-0003-0293-2082; Bailey, Sean/0000-0001-8339-9763 NR 44 TC 140 Z9 141 U1 2 U2 11 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 AUG 1 PY 2007 VL 46 IS 22 BP 5068 EP 5082 DI 10.1364/AO.46.005068 PG 15 WC Optics SC Optics GA 206EQ UT WOS:000249167100031 PM 17676117 ER PT J AU Kuzmanoski, M Box, MA Schmid, B Russell, PB Redemann, J AF Kuzmanoski, Maja Box, Michael A. Schmid, Beat Russell, Philip B. Redemann, Jens TI Case study of modeled aerosol optical properties during the SAFARI 2000 campaign SO APPLIED OPTICS LA English DT Article ID SINGLE-SCATTERING ALBEDO; SOUTHERN AFRICA; SIZE DISTRIBUTIONS; LIGHT-ABSORPTION; WAVELENGTH DEPENDENCE; RADIATIVE PROPERTIES; SKY RADIANCE; DRY SEASON; IN-SITU; PARTICLES AB We present modeled aerosol optical properties (single scattering albedo, asymmetry parameter, and lidar ratio) in two layers with different aerosol loadings and particle sizes, observed during the Southern African Regional Science Initiative 2000 (SAFARI 2000) campaign. The optical properties were calculated from aerosol size distributions retrieved from aerosol layer optical thickness spectra, measured using the NASA Ames airborne tracking 14-channel sunphotometer (AATS-14) and the refractive index based on the available information on aerosol chemical composition. The study focuses on sensitivity of modeled optical properties in the 0.3-1.5 mu m wavelength range to assumptions regarding the mixing scenario. We considered two models for the mixture of absorbing and nonabsorbing aerosol components commonly used to model optical properties of biomass burning aerosol: a layered sphere with absorbing core and nonabsorbing shell and the Maxwell-Garnett effective medium model. In addition, comparisons of modeled optical properties with the measurements are discussed. We also estimated the radiative effect of the difference in aerosol absorption implied by the large difference between the single scattering albedo values (similar to 0.1 at midvisible wavelengths) obtained from different measurement methods for the case with a high amount of biomass burning particles. For that purpose, the volume fraction of black carbon was varied to obtain a range of single scattering albedo values (0.81-0.91 at lambda = 0.50 mu m). The difference in absorption resulted in a significant difference in the instantaneous radiative forcing at the surface and the top of the atmosphere (TOA) and can result in a change of the sign of the aerosol forcing at TOA from negative to positive. (C) 2007 Optical Society of America. C1 Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. Bay Area Environm Res Inst, Sonoma, CA 95476 USA. Pacific NW Natl Lab, MSIN, Richland, WA 99352 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kuzmanoski, M (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. EM mkuzm@phys.unsw.edu.au NR 56 TC 0 Z9 3 U1 0 U2 3 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 AUG 1 PY 2007 VL 46 IS 22 BP 5263 EP 5275 DI 10.1364/AO.46.005263 PG 13 WC Optics SC Optics GA 206EQ UT WOS:000249167100054 PM 17676140 ER PT J AU Beegle, LW Wilson, MG Abilleira, F Jordan, JF Wilson, GR AF Beegle, Luther W. Wilson, Michael G. Abilleira, Fernando Jordan, James F. Wilson, Gregory R. TI A concept for NASA's mars 2016 astrobiology field laboratory SO ASTROBIOLOGY LA English DT Article ID MARTIAN SURFACE-CHEMISTRY; SEDIMENTARY-ROCKS; ORGANIC-COMPOUNDS; MERIDIANI-PLANUM; HABITABLE ZONES; PILBARA CRATON; SOUTH-AFRICA; METHANE; LIFE; SEARCH AB The Mars Program Plan includes an integrated and coordinated set of future candidate missions and investigations that meet fundamental science objectives of NASA and the Mars Exploration Program ( MEP). At the time this paper was written, these possible future missions are planned in a manner consistent with a projected budget profile for the Mars Program in the next decade (2007-2016). As with all future missions, the funding profile depends on a number of factors that include the exact cost of each mission as well as potential changes to the overall NASA budget. In the current version of the Mars Program Plan, the Astrobiology Field Laboratory (AFL) exists as a candidate project to determine whether there were ( or are) habitable zones and life, and how the development of these zones may be related to the overall evolution of the planet. The AFL concept is a surface exploration mission equipped with a major in situ laboratory capable of making significant advancements toward the Mars Program's life-related scientific goals and the overarching Vision for Space Exploration. We have developed several concepts for the AFL that fit within known budget and engineering constraints projected for the 2016 and 2018 Mars mission launch opportunities. The AFL mission architecture proposed here assumes maximum heritage from the 2009 Mars Science Laboratory (MSL). Candidate payload elements for this concept were identified from a set of recommendations put forth by the Astrobiology Field Laboratory Science Steering Group ( AFL SSG) in 2004, for the express purpose of identifying overall rover mass and power requirements for such a mission. The conceptual payload includes a Precision Sample Handling and Processing System that would replace and augment the functionality and capabilities provided by the Sample Acquisition Sample Processing and Handling system that is currently part of the 2009 MSL platform. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Beegle, LW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Luther.Beegle@jpl.nasa.gov RI Beegle, Luther/A-6354-2010 NR 80 TC 13 Z9 15 U1 1 U2 13 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 AUG PY 2007 VL 7 IS 4 BP 545 EP 577 DI 10.1089/ast.2007.0153 PG 33 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 205WC UT WOS:000249144300001 PM 17723090 ER PT J AU Schwarz, GJ Woodward, CE Bode, MF Evans, A Eyres, SP Geballe, TR Gehrz, RD Greenhouse, MA Helton, LA Liller, W Lyke, JE Lynch, DK O'Brien, TJ Rudy, RJ Russell, RW Shore, SN Starrfield, SG Temm, T Truran, JW Venturini, CC Wagner, RM Williams, RE Zamanov, R AF Schwarz, G. J. Woodward, C. E. Bode, M. F. Evans, A. Eyres, S. P. Geballe, T. R. Gehrz, R. D. Greenhouse, M. A. Helton, L. A. Liller, W. Lyke, J. E. Lynch, D. K. O'Brien, T. J. Rudy, R. J. Russell, R. W. Shore, S. N. Starrfield, S. G. Temm, T. Truran, J. W. Venturini, C. C. Wagner, R. M. Williams, R. E. Zamanov, R. TI The early spectrophotometric evolution of V1186 Scorpii (nova Scorpii 2004 no. 1) SO ASTRONOMICAL JOURNAL LA English DT Article DE stars : dwarf novae; stars : individual (V1186 Sco) ID SPITZER-SPACE-TELESCOPE; INFRARED PHOTOMETRY; ABUNDANCE ANALYSIS; CLASSICAL NOVAE; VULPECULAE 1984; PW VULPECULAE; LIGHT-CURVE; NEON NOVA; SPECTROGRAPH; MICRON AB We report optical photometry and optical through mid-infrared spectroscopy of the classical nova V1186 Sco.This slowly developing nova had a complex light curve with multiple secondary peaks similar to those seen in PW Vul. The time to decline 2 mag, t(2) was 20 days, but the erratic nature of the light curve makes determination of intrinsic properties based on the decline time (e.g., luminosity) problematic, and the often-cited relationship of maximum magnitude versus the rate of decay of the light curve of Della Valle & Livio fails to yield a plausible distance. Spectra covering 0.35-35 pm were obtained in two separate epochs during the first year of outburst. The first set of spectra, taken about 2 months after visible maximum, are typical of a CO-type nova with narrow-line emission from HI, Fe II, OI, and He I. Later data, obtained between 260 and 380 days after maximum, reveal an emerging nebular spectrum. Spitzer spectra show weakening hydrogen recombination emission with the emergence of [Ne II] (12.81 mu m) as the strongest line. Strong emission from [Ne in] (15.56 mu,m) is also detected. Photoionization models with low effective temperature sources and only marginal neon enhancement (Ne similar to 1.3 Neo) are consistent with these IR finestructure neon lines indicating that V1186 Sco did not occur on a ONeMg white dwarf. In contrast, the slow and erratic light-curve evolution, spectral development, and photoionization analysis of the ejecta imply that the outburst occurred on a low-mass CO white dwarf. We note that this is the first time strong [Ne II] lines have been detected so early in the outburst of a CO nova and suggest that the presence of mid-infrared neon lines is not directly indicative of a ONeMg nova event. C1 W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. Univ Minnesota, Sch Phys & Astron, Dept Astron, Minneapolis, MN 55455 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. Univ Cent Lancashire, Dept Phys Astron & Math, Preston PR1 2HE, Lancs, England. Gemini Observ, Hilo, HI 96720 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Inst Nova Studies, Vina Del Mar, Chile. WM Keck Observ, Kamuela, HI 96743 USA. Aerosp Corp, Los Angeles, CA 90009 USA. Univ Manchester, Jodrell Bank, Macclesfield SK11 9DL, Cheshire, England. Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy. Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Argonne Natl Lab, Argonne, IL 60437 USA. Univ Arizona, Large Binocular Telescope Observ, Argonne, IL 60437 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Schwarz, GJ (reprint author), W Chester Univ, Dept Geol & Astron, 750 S Church St, W Chester, PA 19383 USA. EM gschwarz@pha.jhu.edu OI Schwarz, Gregory/0000-0002-0786-7307; Temim, Tea/0000-0001-7380-3144 NR 56 TC 10 Z9 10 U1 0 U2 3 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 AUG PY 2007 VL 134 IS 2 BP 516 EP 526 DI 10.1086/519240 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 197XY UT WOS:000248591800006 ER PT J AU Hammel, HB Sitko, ML Lynch, DK Orton, GS Russell, RW Geballe, TR De Pater, I AF Hammel, H. B. Sitko, Mike L. Lynch, David K. Orton, G. S. Russell, R. W. Geballe, T. R. De Pater, Imke TI Distribution of ethane and methane emission on Neptune SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : solar system; planets and satellites : individual (Neptune) ID ADAPTIVE-OPTICS SYSTEM; INFRARED OBSERVATIONS; URANUS; STRATOSPHERE; TEMPERATURE; VARIABILITY; ABUNDANCES; TELESCOPE AB We present the first published spatially resolved images of Neptune's thermal emission. Our 7.7 and 11.7 Am images, taken on 2005 July 4 and 5 at the Gemini North telescope, show enhanced methane and ethane emission within 30 of the south pole. This bright polar region is the first direct imaging evidence for radiative forcing of Neptune's stratosphere, similar to that seen on Saturn. Enhanced emission from ethane, but not methane, also emerges from the planetary limb, suggesting differing vertical profiles. Stratospheric emissions are uncorrelated with tropospheric clouds seen in reflected sunlight in our near-simultaneous adaptive optics images at 1.6 and 2.2 mu m taken with the Keck II telescope on 2005 July 5. C1 Space Sci Inst, Boulder, CO 80301 USA. Aerosp Corp, Los Angeles, CA 90009 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Gemini Observ, Hilo, HI 96720 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Hammel, HB (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. EM hbh@alum.mit.edu NR 26 TC 18 Z9 18 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2007 VL 134 IS 2 BP 637 EP 641 DI 10.1086/519382 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 197XY UT WOS:000248591800016 ER PT J AU Perri, M Guetta, D Antonelli, LA Cucchiara, A Mangano, V Reeves, J Angelini, L Beardmore, AP Boyd, P Burrows, DN Campana, S Capalbi, M Chincarini, G Cusumano, G Giommi, P Hill, JE Holland, ST La Parola, V Mineo, T Moretti, A Nousek, JA Osborne, JP Pagani, C Romano, P Roming, PWA Starling, RLC Tagliaferri, G Troja, E Vetere, L Gehrels, N AF Perri, M. Guetta, D. Antonelli, L. A. Cucchiara, A. Mangano, V. Reeves, J. Angelini, L. Beardmore, A. P. Boyd, P. Burrows, D. N. Campana, S. Capalbi, M. Chincarini, G. Cusumano, G. Giommi, P. Hill, J. E. Holland, S. T. La Parola, V. Mineo, T. Moretti, A. Nousek, J. A. Osborne, J. P. Pagani, C. Romano, P. Roming, P. W. A. Starling, R. L. C. Tagliaferri, G. Troja, E. Vetere, L. Gehrels, N. TI The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; X-rays : individuals : GRB050730 ID BURST AFTERGLOWS; REFRESHED SHOCKS; XRT OBSERVATIONS; ENGINE ACTIVITY; LIGHT CURVES; TELESCOPE; EMISSION; SPECTRA; FLARES; ENERGETICS AB Aims. We observed the high redshift (z = 3.969) GRB 050730 with Swift and XMM-Newton to study its prompt and afterglow emission. Methods. We carried out a detailed spectral and temporal analysis of Swift and XMM-Newton observations. Results. The X-ray afterglow of GRB 050730 was found to decline along with time with superimposed intense flaring activity that extended over more than two orders of magnitude in time. Seven distinct re-brightening events starting from 236 s and up to 41.2 ks after the burst were observed. The underlying decay of the afterglow was well described by a double broken power-law model with breaks at t(1) = 237 +/- 20 s and t(2) = 10.1(-2.2)(+4.6) ks. The temporal decay slopes before, between and after these breaks were alpha(1) = 2.1 +/- 0.3, alpha(2) = 0.44(-0.08)(+0.14) and alpha(3) = 2.40(-0.07)(+0.09) , respectively. The spectrum of the X-ray afterglow was well described by a photoelectrically absorbed power-law with an absorbing column density N-H(z)=(1.28(-0.25)(+0.26)) x 10(22) cm(-2) in the host galaxy. Evidence was found of flaring activity in the early UVOT optical afterglow, simultaneous with that observed in the X-ray band. Strong X-ray spectral evolution during the flaring activity was present. The rise and decay power-law slopes of the first three flares were in the range 0.8-1.8 using as zero times the beginning and the peak of the flares, respectively. In the majority of flares (6/7), the ratio Delta t/t(p) between the duration of the event and the time when the flare peaks was nearly constant and similar to 0.6-0.7. We showed that the observed spectral and temporal properties of the first three flares are consistent with being due both to high-latitude emission, as expected if the flares were produced by late internal shocks, and to refreshed shocks, i.e. late time energy injections into the main afterglow shock by slow moving shells ejected from the central engine during the prompt phase. The event fully satisfies the E-p-E-iso Amati relation but is not consistent with the E-p vs. E-jet Ghirlanda relation. C1 ASI Sci Data Ctr, I-00044 Frascati, Italy. INAF, Astron Observ, I-00040 Rome, Italy. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. INAF, Ist Astrofis Spaziale & Fis Cosm, Sez Palermo, I-90146 Palermo, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. INAF, Astron Observ Brera, I-23807 Merate, Italy. Univ Studi Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. Unita Osserv Univ, Agenzia Spaziale Italiana, I-00198 Rome, Italy. Univ Space Res Assoc, Columbia, MD 21044 USA. RP Perri, M (reprint author), ASI Sci Data Ctr, Via Galileo Galilei, I-00044 Frascati, Italy. EM perri@asdc.asi.it RI Boyd, Patricia/D-3274-2012; Gehrels, Neil/D-2971-2012; OI Mineo, Teresa/0000-0002-4931-8445; guetta, dafne/0000-0002-7349-1109; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315; Perri, Matteo/0000-0003-3613-4409; La Parola, Valentina/0000-0002-8087-6488; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 78 TC 15 Z9 15 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2007 VL 471 IS 1 BP 83 EP 92 DI 10.1051/0004-6361:20066227 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 195ED UT WOS:000248394400014 ER PT J AU Ashdown, MAJ Baccigalupi, C Balbi, A Bartlett, JG Borrill, J Cantalupo, C de Gasperis, G Gorski, KM Heikkila, V Hivon, E Keihanen, E Kurki-Suonio, H Lawrence, CR Natoli, P Poutanen, T Prunet, S Reinecke, M Stompor, R Wandelt, B AF Ashdown, M. A. J. Baccigalupi, C. Balbi, A. Bartlett, J. G. Borrill, J. Cantalupo, C. de Gasperis, G. Gorski, K. M. Heikkila, V. Hivon, E. Keihanen, E. Kurki-Suonio, H. Lawrence, C. R. Natoli, P. Poutanen, T. Prunet, S. Reinecke, M. Stompor, R. Wandelt, B. CA Planck CTP Working Grp TI Making maps from planck LFI 30 GHz data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : cosmic microwave background; methods : data analysis; techniques : image processing; cosmology : observations ID GALACTIC DUST EMISSION; POLARIZED EMISSION; CMB EXPERIMENTS; LATITUDES; SPHERE AB This paper is one of a series describing the performance and accuracy of map-making codes as assessed by the Planck CTP working group. We compare the performance of multiple codes written by different groups for making polarized maps from Planck-sized, all-sky cosmic microwave background (CMB) data. Three of the codes are based on a destriping algorithm, whereas the other three are implementations of a maximum-likelihood algorithm. Previous papers in the series described simulations at 100 GHz (Poutanen et al. 2006, A & A, 449, 1311) and 217 GHz (Ashdown et al. 2007, A & A, 467, 761). In this paper we make maps (temperature and polarisation) from the simulated one-year observations of four 30 GHz detectors of Planck Low Frequency Instrument (LFI). We used Planck Level S simulation pipeline to produce the observed time-ordered-data streams (TOD). Our previous studies considered polarisation observations for the CMB only. For this paper we increased the realism of the simulations and included polarized galactic foregrounds in our sky model, which is based on the version 0.1 of the PLANCK reference sky. Our simulated TODs comprised dipole, CMB, diffuse galactic emissions, extragalactic radio sources, and detector noise. The strong subpixel signal gradients arising from the foreground signals couple to the output map through the map-making and cause an error (signal error) in the maps. Destriping codes have smaller signal error than the maximum-likelihood codes. We examined a number of schemes to reduce this error. On the other hand, the maximum-likelihood map-making codes can produce maps with lower residual noise than destriping codes. C1 Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. Inst Astron, Cambridge CB3 0HA, England. Univ Heidelberg, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. SISSA, ISAS, I-34127 Trieste, Italy. Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. Univ Paris 07, Observ Paris, CEA, Lab Astroparticule & Cosmol, F-75205 Paris, France. Univ Paris 07, Observ Paris, CNRS, UMR 7164, F-75205 Paris, France. Lawrence Berkeley Lab, Computat Res Div, Berkeley, CA 94720 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Pasadena, CA 91125 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Univ Helsinki, Dept Phys Sci, FIN-00014 Helsinki, Finland. Univ Helsinki, Dept Phys Sci, FIN-00014 Helsinki, Finland. Helsinki Inst Phys, FIN-00014 Helsinki, Finland. Inst Astrophys Paris, Paris, France. Max Planck Inst Astrophys, D-85741 Garching, Germany. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Ashdown, MAJ (reprint author), Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. RI de Gasperis, Giancarlo/C-8534-2012; Kurki-Suonio, Hannu/B-8502-2016; OI de Gasperis, Giancarlo/0000-0003-2899-2171; Kurki-Suonio, Hannu/0000-0002-4618-3063; WANDELT, Benjamin/0000-0002-5854-8269; Hivon, Eric/0000-0003-1880-2733 NR 30 TC 20 Z9 20 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2007 VL 471 IS 1 BP 361 EP 380 DI 10.1051/0004-6361:20077312 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 195ED UT WOS:000248394400046 ER PT J AU Godet, O Page, KL Osborne, J Zhang, B Burrows, DN O'Brien, PT Hill, JE Racusin, J Beardmore, AP Goad, MR Falcone, A Morris, DC Ziaeepour, H AF Godet, O. Page, K. L. Osborne, J. Zhang, B. Burrows, D. N. O'Brien, P. T. Hill, J. E. Racusin, J. Beardmore, A. P. Goad, M. R. Falcone, A. Morris, D. C. Ziaeepour, H. TI GRB050822: detailed analysis of an XRF observed by Swift SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; radiation mechanisms : thermal; X-rays : bursts; accretion, accretion disks; miscellaneous ID GAMMA-RAY-BURSTS; ULTRARELATIVISTIC SHOCKS; PARTICLE-ACCELERATION; SPECTRAL-ANALYSIS; ENGINE ACTIVITY; JET MODEL; FLASHES; AFTERGLOW; TELESCOPE; MISSION AB We report on the temporal and spectral characteristics of the early X-ray emission from the GRB 050822 as observed by Swift. This burst is likely to be an XRF showing major X-ray flares in its XRT light-curve. The quality of the data allows a detailed spectral analysis of the early afterglow in the X-ray band. During the X-ray flares, a positive correlation between the count rate and the spectral hardness (i. e. the higher the count rate, the harder the spectrum) is clearly seen for the X-ray flares. This behaviour, similar to that seen for Gamma-ray pulses, indicates that the energy peak of the spectrum is in the XRT energy band and it moves towards lower energies with time. We show evidence for the possible detection of the emergence of the forward-shock emission, produced at a radius larger than 4 x 1016 cm in the case of a CBMafterglow model (a formation region clearly different from that producing the prompt emission). Finally, we show that the null detection of a jet break up to T(0) + 4 x 10(6) s in the X-ray light curve of this XRF can be understood: i) if the jet seen on-axis is uniform with a large opening angle (theta > 20.); or ii) if the jet is a structured Gaussian- like C1 Univ Leicester, Dept Phys & Astron, X Ray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Godet, O (reprint author), Univ Leicester, Dept Phys & Astron, X Ray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. EM og19@star.le.ac.uk RI Racusin, Judith/D-2935-2012 NR 84 TC 11 Z9 11 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2007 VL 471 IS 2 BP 385 EP 394 DI 10.1051/0004-6361:20077266 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 197HR UT WOS:000248545700009 ER PT J AU Cox, NLJ Cordiner, MA Ehrenfreund, P Kaper, L Sarre, PJ Foing, BH Spaans, M Cami, J Sofia, UJ Clayton, GC Gordon, KD Salama, F AF Cox, N. L. J. Cordiner, M. A. Ehrenfreund, P. Kaper, L. Sarre, P. J. Foing, B. H. Spaans, M. Cami, J. Sofia, U. J. Clayton, G. C. Gordon, K. D. Salama, F. TI Interstellar gas, dust and diffuse bands in the SMC SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE astrochemistry; galaxies : Magellanic Clouds; ISM : dust; extinction; ISM : lines and bands; ISM : molecules; ISM : atoms ID SMALL-MAGELLANIC-CLOUD; POLYCYCLIC AROMATIC-HYDROCARBONS; FAR-ULTRAVIOLET EXTINCTION; EARLY-TYPE STARS; SIGHT LINES; ABSORPTION-LINES; MILKY-WAY; CA-II; NA-I; APERTURE SYNTHESIS AB Aims. In order to gain new insight into the unidentified identity of the diffuse interstellar band (DIB) carriers, this paper describes research into possible links between the shape of the interstellar extinction curve ( including the 2175 angstrom bump and far-UV rise), the presence or absence of DIBs, and physical and chemical conditions of the diffuse interstellar medium ( gas and dust) in the Small Magellanic Cloud (SMC). Methods. We searched for DIB absorption features in VLT/UVES spectra of early-type stars in the SMC whose reddened lines-of-sight probe the diffuse interstellar medium of the SMC. Apparent column density profiles of interstellar atomic species (Na I, KI, Ca II and Ti II) are constructed to provide information on the distribution and conditions of the interstellar gas. Results. The characteristics of eight DIBs detected toward the SMC wing target AzV 456 are studied and upper limits are derived for the DIB equivalent widths toward the SMC stars AzV 398, AzV 214, AzV 18, AzV 65 and Sk 191. The amount of reddening is derived for these SMC sightlines, and, using R-V and the Hi column density, converted into a gas-to-dust ratio. From the atomic column density ratios we infer an indication of the strength of the interstellar radiation field, the titanium depletion level and a relative measure of turbulence/ quiescence. The presence or absence of DIBs appears to be related to the shape of the extinction curve, in particular with respect to the presence or absence of the 2175 angstrom feature. Our measurements indicate that the DIB characteristics depend on the local physical conditions and chemical composition of the interstellar medium of the SMC, which apparently determine the rate of formation (and/or) destruction of the DIB carriers. The UV radiation field ( via photoionisation and photo-destruction) and the metallicity (i.e. carbon abundance) are important factors in determining diffuse band strengths which can differ greatly both between and within galaxies. C1 European Space Astron Ctr, Res & Sci Support Dept ESA, Herschel Sci Ctr, Madrid 28080, Spain. Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. Univ Nottingham, Sch Chem, Nottingham NG7 2RD, England. Leiden Univ, Leiden Inst Chem, Astrobiol Grp, NL-2300 RA Leiden, Netherlands. Univ Amsterdam, Astron Inst, NL-1098 SJ Amsterdam, Netherlands. ESTEC, ESA SCI SR, NL-2200 AG Noordwijk, Netherlands. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. SETI Inst, Mountain View, CA 94043 USA. Whitman Coll, Astron Dept, Walla Walla, WA 99362 USA. Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NASA Ames Res Ctr, Space Sci Div, Moffett Field, CA 94035 USA. RP Cox, NLJ (reprint author), European Space Astron Ctr, Res & Sci Support Dept ESA, Herschel Sci Ctr, Ap Correos 50727, Madrid 28080, Spain. EM Nick.Cox@esa.int RI Salama, Farid/A-8787-2009 OI Salama, Farid/0000-0002-6064-4401 NR 119 TC 41 Z9 42 U1 3 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2007 VL 470 IS 3 BP 941 EP U87 DI 10.1051/0004-6361:20065261 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 192HE UT WOS:000248190700013 ER PT J AU Kuo, CL Ade, PAR Bock, JJ Bond, JR Contaldi, CR Daub, MD Goldstein, JH Holzapfel, WL Lange, AE Lueker, M Newcomb, M Peterson, JB Reichardt, C Ruhl, J Runyan, MC Staniszweski, Z AF Kuo, C. L. Ade, P. A. R. Bock, J. J. Bond, J. R. Contaldi, C. R. Daub, M. D. Goldstein, J. H. Holzapfel, W. L. Lange, A. E. Lueker, M. Newcomb, M. Peterson, J. B. Reichardt, C. Ruhl, J. Runyan, M. C. Staniszweski, Z. TI Improved measurements of the CMB power spectrum with ACBAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations ID COSMIC BACKGROUND IMAGER; PROBE WMAP OBSERVATIONS; GALAXY REDSHIFT SURVEY; 2003 FLIGHT; COSMOLOGICAL PARAMETERS; NUMBER COUNTS; LOCKMAN HOLE; MOSAIC OBSERVATIONS; MICROWAVE; ANISOTROPY AB We report improved measurements of temperature anisotropies in the cosmic microwave background (CMB) radiation made with the Arcminute Cosmology Bolometer Array Receiver (ACBAR). In this paper, we use a new analysis technique and include 30% more data from the 2001 and 2002 observing seasons than the first release to derive a new set of band-power measurements with significantly smaller uncertainties. The planet-based calibration used previously has been replaced by comparing the flux of RCW38 as measured by ACBAR and BOOMERANG to transfer the WMAP-based BOOMERANG calibration to ACBAR. The resulting power spectrum is consistent with the theoretical predictions for a spatially flat, dark energy-dominated Lambda CDM cosmology, including the effects of gravitational lensing. Despite the exponential damping on small angular scales, the primary CMB fluctuations are detected with a signal-to-noise ratio of greater than 4, up to multipoles of l = 2000. This increase in the precision of the fine-scale CMB power spectrum leads to only a modest decrease in the uncertainties on the parameters of the standard cosmological model. At high angular resolution, secondary anisotropies are predicted to be a significant contribution to the measured anisotropy. A joint analysis of the ACBAR results at 150 GHz and the CBI results at 30 GHz in the multipole range 2000 < l < 3000 shows that the power, reported by CBI in excess of the predicted primary anisotropy, has a frequency spectrum consistent with the thermal Sunyaev-Zel'dovich effect and inconsistent with primary CMB. The results reported here are derived from a subset of the total ACBAR data set; the final ACBAR power spectrum at 150 GHz will include 3.7 times more effective integration time and 6.5 times more sky coverage than is used here. C1 CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, Wales. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Univ Chicago, Dept Phys, Chicago, IL 60637 USA. RP Kuo, CL (reprint author), CALTECH, MS 59-33, Pasadena, CA 91125 USA. RI Peterson, Jeffrey/O-4794-2014; Holzapfel, William/I-4836-2015; OI Peterson, Jeffrey/0000-0003-1340-818X; Reichardt, Christian/0000-0003-2226-9169 NR 64 TC 60 Z9 60 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 AUG 1 PY 2007 VL 664 IS 2 BP 687 EP 701 DI 10.1086/518401 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000009 ER PT J AU Sajina, A Yan, L Armus, L Choi, P Fadda, D Helou, G Spoon, H AF Sajina, Anna Yan, Lin Armus, Lee Choi, Philip Fadda, Dario Helou, George Spoon, Henrik TI Spitzer mid-infrared spectroscopy of infrared luminous galaxies at z similar to 2. II. Diagnostics SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : high-redshift; infrared : galaxies ID ACTIVE GALACTIC NUCLEI; POLYCYCLIC AROMATIC-HYDROCARBON; DIFFUSE INTERSTELLAR-MEDIUM; STAR-FORMING GALAXIES; QUASAR HOST GALAXIES; SPACE-TELESCOPE; SUBMILLIMETER GALAXIES; CRYSTALLINE SILICATES; IRS SPECTROSCOPY; SPECTRA AB We present mid-IR spectral decomposition of a sample of 48 Spitzer-selected ULIRGs spanning z similar to 1-3 and likely L-IR similar to 10(12)-10(13) L-circle dot. Our study aims at quantifying the star formation and active galactic nucleus (AGN) processes in these sources that recent results suggest have evolved strongly between the observed epoch and today. To do this, we study the mid-IR contribution of PAH emission, continuum, and extinction. About 3/4 of our sample are continuum (i.e., AGN) dominated sources, but similar to 60% of these show PAH emission, suggesting the presence of star formation activity. These sources have redder mid-IR colors than typical optically selected quasars. About 25% of our sample have strong PAH emission, but none are likely to be pure starbursts as reflected in their relatively high 5 mu m hot dust continua. However, their steep 30-14 mu m slopes suggest that star formation might dominate the total infrared luminosity. Six of our z similar to 2 sources have EW6.2 greater than or similar to 0.3 mu m and L-14 mu m greater than or similar to 10(12) L-circle dot (implying L-IR greater than or similar to 10(13) L-circle dot). At these luminosities, such high EW6.2 ULIRGs do not exist in the local universe. We find a median optical depth at 9.7 mu m of = 1.4. This is consistent with local IRAS-selected ULIRGs but differs from early results on SCUBA-selected z similar to 2 ULIRGs. Similar to local ULIRGs, about 25% of our sample shows extreme obscuration (tau(9.7 mu m) greater than or similar to 3), suggesting buried nuclei. In general, we find that our sources are similar to local ULIRGs but are an order of magnitude more luminous. It is not clear whether our z similar to 2 ULIRGs are simply scaled-up versions of local ULIRGs or subject to fundamentally different physical processes. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Pomona Coll, Claremont, CA 91711 USA. CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. Cornell Univ, Ithaca, NY 14853 USA. RP Sajina, A (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. NR 64 TC 129 Z9 128 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2007 VL 664 IS 2 BP 713 EP 737 DI 10.1086/519446 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000011 ER PT J AU Huang, JS Ashby, MLN Barmby, P Brodwin, M Brown, MJI Caldwell, N Cool, RJ Eisenhardt, P Eisenstein, D Fazio, GG Le Floc'h, E Green, P Kochanek, CS Lu, N Pahre, MA Rigopoulou, D Rosenberg, JL Smith, HA Wang, Z Willmer, CNA Willner, SP AF Huang, J.-S. Ashby, M. L. N. Barmby, P. Brodwin, M. Brown, M. J. I. Caldwell, N. Cool, R. J. Eisenhardt, P. Eisenstein, D. Fazio, G. G. Le Floc'h, E. Green, P. Kochanek, C. S. Lu, Nanyao Pahre, M. A. Rigopoulou, D. Rosenberg, J. L. Smith, H. A. Wang, Z. Willmer, C. N. A. Willner, S. P. TI The local galaxy 8 mu m luminosity function SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; dust, extinction; galaxies : luminosity function, mass function; infrared : galaxies ID SPITZER-SPACE-TELESCOPE; ULTRALUMINOUS INFRARED GALAXIES; POLYCYCLIC AROMATIC-HYDROCARBON; HUBBLE-DEEP-FIELD; FIBER-FED SPECTROGRAPH; STAR-FORMING GALAXIES; IR EMISSION FEATURES; ARRAY CAMERA IRAC; RED GALAXIES; REDSHIFT SURVEY AB A Spitzer Space Telescope survey in the NOAO Deep Wide Field in Bootes provides a complete, 8 mu m-selected sample of galaxies to a limiting (Vega) magnitude of 13.5. In the 6.88 deg(2) field sampled, 79% of the 4867 galaxies have spectroscopic redshifts, allowing an accurate determination of the local (z < 0.3) galaxy luminosity function. Stellar and dust emission can be separated on the basis of observed galaxy colors. Dust emission (mostly PAH) accounts for 80% of the 8 mu m luminosity, stellar photospheres account for 19%, and AGN emission accounts for roughly 1%. A subsample of the 8 mu m-selected galaxies have blue, early-type colors, but even most of these have significant PAH emission. The luminosity functions for the total 8 mu m luminosity and for the dust emission alone are both well fit by Schechter functions. For the 8 mu m luminosity function, the characteristic luminosity is vL(v)*(8.0 mu m) = 1.8 x 10(10) L(circle dot), while for the dust emission alone it is 1.6 x 10(10) L(circle dot). The average 8 mu m luminosity density at z < 0.3 is 3.1 x 10(7) L(circle dot) Mpc(-3), and the average luminosity density from dust alone is 2.5 x 10(7) L(circle dot) Mpc(-3). This luminosity arises predominantly from galaxies with 8 mu m luminosities (vL(v)) between 2 x 10(9) and 2 x 10(10) L(circle dot), i.e., normal galaxies, not luminous or ultraluminous infrared galaxies (LIRGs/ULIRGs). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. RP Huang, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Brown, Michael/B-1181-2015; Barmby, Pauline/I-7194-2016 OI Brown, Michael/0000-0002-1207-9137; Barmby, Pauline/0000-0003-2767-0090 NR 81 TC 48 Z9 48 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 AUG 1 PY 2007 VL 664 IS 2 BP 840 EP 849 DI 10.1086/519241 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000019 ER PT J AU Neufeld, DA Hollenbach, DJ Kaufman, MJ Snell, RL Melnick, GJ Bergin, EA Sonnentrucker, P AF Neufeld, David A. Hollenbach, David J. Kaufman, Michael J. Snell, Ronald L. Melnick, Gary J. Bergin, Edwin A. Sonnentrucker, Paule TI Spitzer spectral line mapping of supernova remnants. I. Basic data and principal component analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : clouds; ISM : molecules; molecular processes; shock waves ID SHOCKED MOLECULAR GAS; 3C 391; INTERSTELLAR-MEDIUM; INFRARED-SPECTROSCOPY; NOVA REMNANT; X-RAY; ROTATIONAL LINES; IC-443; W28; W44 AB We report the results of spectroscopic mapping observations carried out toward small (1' x 1') regions within the supernova remnants W44, W28, IC 443, and 3C 391 using the Infrared Spectrograph (IRS) of the Spitzer Space Telescope. These observations, covering the 5.2-37 mu m spectral region, have led to the detection of a total of 15 fine-structure transitions of Ne+, Ne++, Si+, P+, S, S++, Cl+, Fe+, and Fe++; the S(0)-S(7) pure rotational lines of molecular hydrogen; and the R(3) and R(4) transitions of hydrogen deuteride. In addition to these 25 spectral lines, the 6.2, 7.7, 8.6, 11.3, and 12.6 mu m PAH emission bands were also observed. Most of the detected line transitions have proven strong enough to map in several sources, providing a comprehensive picture of the relative distribution of the various line emissions observable in the Spitzer IRS bandpass. A principal component analysis of the spectral-line maps reveals that the observed emission lines fall into five distinct groups, each of which may exhibit a distinct spatial distribution: (1) lines of S and H-2(J > 2); (2) the H-2 S(0) line; (3) lines of ions with appearance potentials less than 13.6 eV; ( 4) lines of ions with appearance potentials greater than 13.6 eV, not including S++; (5) lines of S++. Lines of group 1 likely originate in molecular material subject to a slow, nondissociative shock that is driven by the overpressure within the supernova remnant, and lines in groups 3-5 are associated primarily with dissociative shock fronts with a range of (larger) shock velocities. The H-2 S(0) line shows a low-density diffuse emission component and, in some sources, a shock-excited component. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. NR 68 TC 45 Z9 45 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2007 VL 664 IS 2 BP 890 EP 908 DI 10.1086/518857 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000023 ER PT J AU Kellogg, E Anderson, C Korreck, K DePasquale, J Nichols, J Sokoloski, JL Krauss, M Pedelty, J AF Kellogg, E. Anderson, C. Korreck, K. DePasquale, J. Nichols, J. Sokoloski, J. L. Krauss, M. Pedelty, J. TI Outer jet X-ray and radio emission in R Aquarii: 1999.8 to 2004.0 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : symbiotic; circumstellar matter; radio continuum : stars; stars : individual (R Aquarii); stars : winds, outflows; white dwarfs; X-rays : general ID CH-CYGNI; PROTOSTELLAR JET; ULTRAVIOLET; SYSTEM; DISCOVERY; SHOCK; SPECTROSCOPY; VARIABILITY; RESOLUTION; OUTBURST AB Chandra and VLA observations of the symbiotic star R Aqr in 2004 reveal significant changes over the 3-4 year interval between these observations and previous observations taken in with the VLA in 1999 and with Chandra in 2000. This paper reports on the evolution of the outer thermal X-ray lobe jets and radio jets. The emission from the outer X-ray lobe jets lies farther away from the central binary than the outer radio jets and comes from material interpreted as being shock-heated to similar or equal to 10(6) K, a likely result of collision between high-speed material ejected from the central binary and regions of enhanced gas density. Between 2000 and 2004, the northeast (NE) outer X-ray lobe jet moved out, away from the central binary, with an apparent projected motion of similar or equal to 580 km s(-1). The southwest (SW) outer X-ray lobe jet almost disappeared between 2000 and 2004, presumably due to adiabatic expansion and cooling. The NE radio-bright spot also moved away from the central binary between 2000 and 2004, but with a smaller apparent velocity than the NE X-ray-bright spot. The SW outer lobe jet was not detected in the radio in either 1999 or 2004. The density and mass of the X-ray-emitting material is estimated. Cooling times, shock speeds, pressure, and confinement are discussed. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RP Kellogg, E (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM ekellogg@cfa.harvard.edu NR 45 TC 21 Z9 21 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2007 VL 664 IS 2 BP 1079 EP 1087 DI 10.1086/518877 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000040 ER PT J AU Furlan, E Sargent, B Calvet, N Forrest, WJ D'Alessio, P Hartmann, L Watson, DM Green, JD Najita, J Chen, CH AF Furlan, E. Sargent, B. Calvet, N. Forrest, W. J. D'Alessio, P. Hartmann, L. Watson, D. M. Green, J. D. Najita, J. Chen, C. H. TI HD 98800: A 10 Myr old transition disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; circumstellar matter; infrared : stars; planetary systems : formation; stars : individual (HD 98800) ID T-TAURI STARS; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; INTERSTELLAR SILICATE MINERALOGY; HYDRAE ASSOCIATION; HD 98800; KUIPER-BELT; INFRARED SPECTROGRAPH; ACCRETION DISK; SYSTEM AB We present the mid-infrared spectrum, obtained with the Spitzer Infrared Spectrograph (IRS), of HD 98800, a quadruple star system located in the 10 Myr old TW Hydrae association. It has a known mid-infrared excess that arises from a circumbinary disk around the B components of the system. The IRS spectrum confirms that the disk around HD 98800B displays no excess emission below about 5.5 mu m, implying an optically thick disk wall at 5.9 AU and an inner, cleared-out region; however, some optically thin dust, consisting mainly of 3 mu m-sized silicate dust grains, orbits the binary in a ring between 1.5 and 2 AU. The peculiar structure and apparent lack of gas in the HD 98800B disk suggests that this system is likely already at the debris disks stage, with a tidally truncated circumbinary disk of larger dust particles and an inner, second-generation dust ring, possibly held up by the resonances of a planet. The unusually large infrared excess can be explained by gravitational perturbations of the Aa+Ab pair puffing up the outer dust ring and causing frequent collisions among the larger particles. C1 Univ Calif Los Angeles, NASA, Astrobiol Inst, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Furlan, E (reprint author), Univ Calif Los Angeles, NASA, Astrobiol Inst, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM furlan@astro.ucla.edu; bsargent@pas.rochester.edu; ncalvet@umich.edu; forrest@pas.rochester.edu; p.dalessio@astrosmo.unam.mx; lhartm@umich.edu; dmw@pas.rochester.edu; joel@pas.rochester.edu; najita@noao.edu; cchen@noao.edu OI Furlan, Elise/0000-0001-9800-6248 NR 49 TC 40 Z9 40 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2007 VL 664 IS 2 BP 1176 EP 1184 DI 10.1086/519301 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000049 ER PT J AU Rauscher, E Menou, K Seager, S Deming, D Cho, JYK Hansen, BMS AF Rauscher, Emily Menou, Kristen Seager, Sara Deming, Drake Cho, James Y. -K. Hansen, Bradley M. S. TI Toward eclipse mapping of hot Jupiters SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; infrared : stars; occultations; planetary systems; stars : individual; (HD 189733, HD 209458, TrES-1); techniques : high angular resolution ID EXTRASOLAR GIANT PLANETS; HD 209458B; TRANSITING PLANET; LIGHT CURVES; THERMAL EMISSION; TRES-1; STAR; ATMOSPHERES; PARAMETERS; HD-189733 AB Recent Spitzer infrared measurements of hot-Jupiter eclipses suggest that eclipse-mapping techniques could be used to spatially resolve the dayside photospheric emission of these planets using partial occultations. As a first step in this direction, we simulate ingress/egress light curves for three bright eclipsing hot Jupiters and evaluate the degree to which parameterized photospheric emission models can be distinguished from each other with repeated, noisy eclipse measurements. We find that the photometric accuracy of Spitzer is insufficient to use this tool effectively. On the other hand, the level of photospheric details that could be probed with a few JWST eclipse measurements could greatly inform hot-Jupiter atmospheric modeling efforts. A JWST program focused on nonparametric eclipse map inversions for hot Jupiters should be actively considered. C1 Columbia Univ, Dept Astron, New York, NY 10027 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. Queen Mary Univ London, Sch Math Sci, Astron Unit, London E1 4NS, England. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, Inst Geophys & Planetary Sci, Los Angeles, CA 90095 USA. RP Rauscher, E (reprint author), Columbia Univ, Dept Astron, 1328 Pupin Hall,550 W 120th St, New York, NY 10027 USA. OI Rauscher, Emily/0000-0003-3963-9672 NR 43 TC 23 Z9 23 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2007 VL 664 IS 2 BP 1199 EP 1209 DI 10.1086/519213 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000052 ER PT J AU Hanasoge, SM Duvall, TL Couvidat, S AF Hanasoge, S. M. Duvall, T. L., Jr. Couvidat, S. TI Validation of helioseismology through forward modeling: Realization noise subtraction and kernels SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; sun : helioseismology; sun : interior; sun : oscillations; waves ID TIME-DISTANCE HELIOSEISMOLOGY; COMPUTATIONAL ACOUSTICS; 3-DIMENSIONAL INVERSION; SENSITIVITY KERNELS; SOUND-SPEED; APPROXIMATION; ABSORPTION; SUNSPOTS; SCHEMES AB Through a series of numerical simulations of the near-surface acoustic wavefield of the Sun, we show the utility of the forward approach in local helioseismology. We demonstrate and apply a method to subtract a large fraction of the realization noise from the simulated data. The ability to attain high signal-to-noise ratios from brief forward calculations implies that computational resources are less of a bottleneck, making this alternate method for investigations of the solar interior very feasible. We put this method to use by deriving sensitivity kernels for sound-speed perturbations and source suppression for the background state in our computations using techniques of time-distance helioseismology, all from merely 48 hr of artificial data. C1 Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA. NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Hanasoge, SM (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM shravan@stanford.edu RI Duvall, Thomas/C-9998-2012 NR 28 TC 30 Z9 30 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 AUG 1 PY 2007 VL 664 IS 2 BP 1234 EP 1243 DI 10.1086/519070 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000057 ER PT J AU Kimura, Y Nuth, JA AF Kimura, Yuki Nuth, Joseph A., III TI What is the driving force to form refractory oxide grains? Silicate spectra depend on their formation environment SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared : general; methods : laboratory; plasmas ID PARTICLES; CONDENSATION; EVOLUTION; ENERGY; IRON AB We discuss room-temperature condensation experiments using either an electrical discharge or ultraviolet radiation to initiate gas-phase reactions resulting in silicate smokes. This formation process could represent processes occurring in low-density environments, because it is possible that the gases, which can condense at higher temperatures, remain after it cools, e. g., following a shock. In these environments, many condensates could be formed simultaneously. However, in the case of our iron silicate experiments, many of the smoke particles are iron silicate with a uniform composition that reflects the composition of the ambient gas atmosphere where they were produced. In these experiments, smoke particles of other materials such as iron oxide and silica were not formed. In the case of our Si-O experiments, hydro-silicate smoke particles are produced together with anhydrous silicate particles directly from the gas phase without later hydro alteration. The infrared spectra of these silicate particles show a very strong 11.36 mu m feature attributed to H2Si2O4 and possibly to Si2O3 compared with a simultaneously observed 9.2 mu m feature due to the Si-O vibration. We believe that finding the driving force for grain growth under a wide range of environmental conditions is important if we are to understand grain formation, because silicate grains, which formed in a plasma field or under UV irradiation, show different compositions, structures, shapes, and spectra from thermally condensed grains. C1 NASA, Goddard Space Flight Ctr, Astrochem Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Kimura, Y (reprint author), Ritsumeikan Univ, Dept Phys, Lab Nano Struct Sci, 1-1-1 Nojihigashi, Kusatsu, Shiga 5258577, Japan. EM ykimura@se.ritsumei.ac.jp RI Nuth, Joseph/E-7085-2012; Kimura, Yuki/J-9635-2014 OI Kimura, Yuki/0000-0002-9218-7663 NR 16 TC 6 Z9 6 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2007 VL 664 IS 2 BP 1253 EP 1263 DI 10.1086/519299 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000059 ER PT J AU Bernstein, MP Sandford, SA Mattioda, AL Allamandola, LJ AF Bernstein, M. P. Sandford, S. A. Mattioda, A. L. Allamandola, L. J. TI Near- and mid-infrared laboratory spectra of PAH cations in solid H(2)O SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; astrochemistry; infrared : ISM; infrared : solar system; ISM : lines and bands; ISM : molecules; methods : laboratory ID POLYCYCLIC AROMATIC-HYDROCARBONS; RADICAL CATIONS; ABSORPTION-SPECTROSCOPY; DEUTERIUM ENRICHMENT; EMBEDDED PROTOSTARS; ORGANIC-MATTER; WATER-ICES; NAPHTHALENE; ANTHRACENE; CLOUDS AB Polycyclic aromatic hydrocarbons (PAHs) have been observed in absorption along lines of sight toward embedded protostars. In such cold space environments PAHs should condense into H(2)O- rich ice mantles at low temperature and be exposed to ionizing radiation. In this paper we present the first infrared spectra of PAH cations in solid H(2)O generated under conditions that resemble dense molecular clouds. After exposing PAHs in solid H(2)O at 15 K to low doses of UV radiation, we have observed both the vibrational absorptions of PAH cations in the mid-IR and electronic transitions in the near-IR. The PAHs observed as ions in solid H(2)O were naphthalene, anthracene, phenanthrene, benzo[k] fluoranthene, and benzo[ghi] perylene. Peak positions, strengths, and temperature dependence are reported for the detected ion bands, and their astrophysical significance is discussed. These laboratory measurements suggest that absorption bands of PAH cations in H(2)O ice may be observable by astronomers in the near- and mid-infrared. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Bernstein, MP (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. EM mbernstein@mail.arc.nasa.gov NR 42 TC 25 Z9 25 U1 1 U2 18 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 AUG 1 PY 2007 VL 664 IS 2 BP 1264 EP 1272 DI 10.1086/518756 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199CY UT WOS:000248675000060 ER PT J AU Abdo, AA Allen, B Berley, D Casanova, S Chen, C Coyne, DG Dingus, BL Ellsworth, RW Fleysher, L Fleysher, R Gonzalez, MM Goodman, JA Hays, E Hoffman, CM Hopper, B Huntemeyer, PH Kolterman, BE Lansdell, CP Linnemann, JT McEnery, JE Mincer, AI Nemethy, P Noyes, D Ryan, JM Parkinson, PMS Shoup, A Sinnis, G Smith, AJ Sullivan, GW Vasileiou, V Walker, GP Williams, DA Xu, XW Yodh, GB AF Abdo, A. A. Allen, B. Berley, D. Casanova, S. Chen, C. Coyne, D. G. Dingus, B. L. Ellsworth, R. W. Fleysher, L. Fleysher, R. Gonzalez, M. M. Goodman, J. A. Hays, E. Hoffman, C. M. Hopper, B. Huentemeyer, P. H. Kolterman, B. E. Lansdell, C. P. Linnemann, J. T. McEnery, J. E. Mincer, A. I. Nemethy, P. Noyes, D. Ryan, J. M. Parkinson, P. M. Saz Shoup, A. Sinnis, G. Smith, A. J. Sullivan, G. W. Vasileiou, V. Walker, G. P. Williams, D. A. Xu, X. W. Yodh, G. B. TI TeV gamma-ray sources from a survey of the Galactic plane with Milagro SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations ID HEGRA IACT-SYSTEM; SURROUNDING FIELD; POINT SOURCES; CRAB-NEBULA; GEMINGA; PULSAR; DISCOVERY; SEARCH AB A survey of Galactic gamma-ray sources at a median energy of similar to 20 TeV has been performed using the Milagro Gamma-Ray Observatory. Eight candidate sources of TeV emission are detected with pretrial significances > 4.5 sigma in the region of Galactic longitude l is an element of [ 30 degrees, 220 degrees] and latitude b is an element of [-10 degrees, 10 degrees]. Four of these sources, including the Crab Nebula and the recently published MGRO J2019 + 37, are observed with significances > 4.5 sigma after accounting for the trials. All four of these sources are also coincident with EGRET sources. Two of the lower significance sources are coincident with EGRET sources, and one of these sources is Geminga. The other two candidates are in the Cygnus region of the Galaxy. Several of the sources appear to be spatially extended. The fluxes of the sources at 20 TeV range from similar to 25% of the Crab flux to nearly as bright as the Crab. C1 Michigan State Univ, E Lansing, MI 48824 USA. Univ Calif Irvine, Irvine, CA USA. Univ Maryland, College Pk, MD 20742 USA. Los Alamos Natl Lab, Los Alamos, NM USA. Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. George Mason Univ, Fairfax, VA 22030 USA. NYU, New York, NY USA. Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ New Hampshire, Durham, NH 03824 USA. Ohio State Univ, Lima, OH 45804 USA. RP Abdo, AA (reprint author), Michigan State Univ, E Lansing, MI 48824 USA. RI McEnery, Julie/D-6612-2012; Hays, Elizabeth/D-3257-2012; Casanova, Sabrina/J-8935-2013; OI Casanova, Sabrina/0000-0002-6144-9122; Dingus, Brenda/0000-0001-8451-7450; Mincer, Allen/0000-0002-6307-1418 NR 28 TC 129 Z9 131 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2007 VL 664 IS 2 BP L91 EP L94 DI 10.1086/520717 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DC UT WOS:000248675400008 ER PT J AU Bhattacharyya, S Strohmayer, TE AF Bhattacharyya, Sudip Strohmayer, Tod E. TI Evidence of a broad relativistic iron line from the neutron star low-mass X-ray binary Serpens X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; line : profiles; relativity; stars : neutron; X-rays : binaries; X-rays : individual (Serpens X-1) ID BLACK-HOLE; GALAXY MCG-6-30-15; RXTE OBSERVATIONS; EMISSION-LINE; LIGHT CURVES; DISK; ABSORPTION; BURSTS; SUZAKU; SPIN AB We report on an analysis of XMM-Newton data from the neutron star low-mass X-ray binary (LMXB) Serpens X-1 (Ser X-1). Spectral analysis of EPIC PN data indicates that the previously known broad iron K alpha emission line from this source has a significantly skewed structure with a moderately extended red wing. The asymmetric shape of the line is well described with the laor and diskline models in XSPEC and strongly supports an inner accretion disk origin of the line. To our knowledge, this is the first strong evidence of a relativistic line in a neutron star LMXB. This finding suggests that the broad lines seen in other neutron star LMXBs likely originate from the inner disk as well. Detailed study of such lines opens up a new way to probe neutron star parameters and their strong gravitational fields. The red wing of the iron line from Ser X-1 is not as broad as that observed from some black hole systems. This is not unreasonable for a neutron star system, as the accretion disk has to terminate at or before the hard stellar surface. Finally, the inferred source inclination angle in the approximate range 40 degrees-60 degrees is consistent with the lack of dips and eclipses from Ser X-1. C1 NASA, Goddard Space Flight Ctr, CRESST, Div Astrophys Sci, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Div Astrophys Sci, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Bhattacharyya, S (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Div Astrophys Sci, Greenbelt, MD 20771 USA. EM sudip@milkyway.gsfc.nasa.gov; stroh@clarence.gsfc.nasa.gov NR 28 TC 54 Z9 54 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 AUG 1 PY 2007 VL 664 IS 2 BP L103 EP L106 DI 10.1086/520844 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DC UT WOS:000248675400011 ER PT J AU Ueda, Y Eguchi, S Terashima, Y Mushotzky, R Tueller, J Markwardt, C Gehrels, N Hashimoto, Y Potter, S AF Ueda, Yoshihiro Eguchi, Satoshi Terashima, Yuichi Mushotzky, Richard Tueller, Jack Markwardt, Craig Gehrels, Neil Hashimoto, Yasuhiro Potter, Stephen TI Suzaku observations of active galactic nuclei detected in the Swift BAT survey: Discovery of a "new type" of buried supermassive black holes SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; gamma rays : observations; X-rays : galaxies; X-rays : general ID HARD X-RAY; SEYFERT 2 GALAXIES; LUMINOSITY FUNCTION; LINE EMISSION; XMM-NEWTON; AGN; ABSORPTION; OBSCURATION; SAMPLE; SKY AB We present the Suzaku broadband observations of two AGNs detected by the Swift BAT hard X-ray (> 15 keV) survey that did not have previous X-ray data, SWIFT J0601.9-8636 and SWIFT J0138.6-4001. The Suzaku spectra reveal in both objects a heavily absorbed power-law component with a column density of N-H similar or equal to 10(23.5) - 10(24) cm(-2) that dominates above 10 keV and an intense reflection component with a solid angle greater than or similar to 2 pi from a cold, optically thick medium. We find that these AGNs have an extremely small fraction of scattered light from the nucleus, less than or similar to 0.5% with respect to the intrinsic power-law component. This indicates that they are buried in a very geometrically thick torus with a small opening angle and/or have an unusually small amount of gas responsible for scattering. In the former case, the geometry of SWIFT J0601.9 - 8636 should be nearly face-on as inferred from the small absorption for the reflection component. The discovery of two such objects in this small sample implies that there must be a significant number of yet unrecognized, very Compton thick AGNs viewed at larger inclination angles in the local universe, which are difficult to detect even in the currently most sensitive optical or hard X-ray surveys. C1 Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. Ehime Univ, Fac Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. S African Astron Observ, ZA-7935 Cape Town, South Africa. RP Ueda, Y (reprint author), Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. RI Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; XRAY, SUZAKU/A-1808-2009 NR 34 TC 102 Z9 102 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 AUG 1 PY 2007 VL 664 IS 2 BP L79 EP L82 DI 10.1086/520576 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DC UT WOS:000248675400005 ER PT J AU Seymour, N Stern, D De Breuck, C Vernet, J Rettura, A Dickinson, M Dey, A Eisenhardt, P Fosbury, R Lacy, M McCarthy, P Miley, G Rocca-Volmerange, B Rottgering, H Stanford, A Teplitz, H van Breugel, W Zirm, A AF Seymour, Nick Stern, Daniel De Breuck, Carlos Vernet, Joel Rettura, Alessandro Dickinson, Mark Dey, Arjun Eisenhardt, Peter Fosbury, Robert Lacy, Mark McCarthy, Pat Miley, George Rocca-Volmerange, Brigitte Roettgering, Huub Stanford, Adam Teplitz, Harry van Breugel, Wil Zirm, Andrew TI The massive hosts of radio galaxies across cosmic time SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE galaxies : active; galaxies : evolution; galaxies : high-redshift ID ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; HUBBLE-DEEP-FIELD; K-Z RELATION; SPECTRAL ENERGY-DISTRIBUTIONS; OLD ELLIPTIC GALAXIES; 7C REDSHIFT SURVEY; LY-ALPHA EMITTERS; BLACK-HOLE MASS; LUMINOSITY FUNCTION AB We present the results of a comprehensive Spitzer survey of 69 radio galaxies across 1 < z < 5.2. Using IRAC ( 3.6-8.0 mu m), IRS ( 16 mu m), and MIPS ( 24-160 mu m) imaging, we decompose the rest-frame optical to infrared spectral energy distributions into stellar, AGN, and dust components and determine the contribution of host galaxy stellar emission at rest-frame Hband. Stellar masses derived from rest-frame near-IR data, where AGN and young star contributions are minimized, are significantly more reliable than those derived from rest-frame optical and UV data. We find that the fraction of emitted light at rest-frame H band from stars is > 60% for similar to 75% of the high-redshift radio galaxies. As expected from unified models of AGNs, the stellar fraction of the rest-frame H-band luminosity has no correlation with redshift, radio luminosity, or rest-frame mid-IR( 5 mu m) luminosity. In addition, while the stellar H-band luminosity does not vary with stellar fraction, the total H-band luminosity anticorrelates with the stellar fraction as would be expected if the underlying hosts of these radio galaxies comprise a homogeneous population. The resultant stellar luminosities imply stellar masses of 10(11)-10(11.5): 5 M-circle dot even at the highest redshifts. Powerful radio galaxies tend to lie in a similar region of mid-IR color-color space as unobscured AGNs, despite the stellar contribution to their mid-IR SEDs at shorter wavelengths. The mid-IR luminosities alone classify most HzRGs as LIRGs or ULIRGs with even higher total-IR luminosities. As expected, these exceptionally high mid-IR luminosities are consistent with an obscured, highly accreting AGN. We find a weak correlation of stellar mass with radio luminosity. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. European So Observ, D-85748 Garching, Germany. Johns Hopkins Univ, Baltimore, MD 21218 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Carnegie Observ, Pasadena, CA 91101 USA. Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. Inst Astrophys, F-75014 Paris, France. Univ Calif Davis, Davis, CA 95616 USA. Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. Univ Calif, Merced, CA 95344 USA. RP Seymour, N (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM seymour@ipac.caltech.edu OI Fosbury, Robert/0000-0001-9975-8003; Vernet, Joel/0000-0002-8639-8560; Seymour, Nicholas/0000-0003-3506-5536; De Breuck, Carlos/0000-0002-6637-3315 NR 123 TC 154 Z9 154 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2007 VL 171 IS 2 BP 353 EP 375 DI 10.1086/517887 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DO UT WOS:000248676600001 ER PT J AU Rebull, LM Stapelfeldt, KR Evans, NJ Jorgensen, JK Harvey, PM Brooke, TY Bourke, TL Padgett, DL Chapman, NL Lai, SP Spiesman, WJ Noriega-Crespo, A Merin, B Huard, T Allen, LE Blake, GA Jarrett, T Koerner, DW Mundy, LG Myers, PC Sargent, AI van Dishoeck, EF Wahhaj, Z Young, KE AF Rebull, L. M. Stapelfeldt, K. R. Evans, N. J., II Jorgensen, J. K. Harvey, P. M. Brooke, T. Y. Bourke, T. L. Padgett, D. L. Chapman, N. L. Lai, S.-P. Spiesman, W. J. Noriega-Crespo, A. Merin, B. Huard, T. Allen, L. E. Blake, G. A. Jarrett, T. Koerner, D. W. Mundy, L. G. Myers, P. C. Sargent, A. I. van Dishoeck, E. F. Wahhaj, Z. Young, K. E. TI The Spitzer c2d survey of large, nearby, interstellar clouds. VI. Perseus observed with MIPS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; infrared : ISM; infrared : stars; ISM : clouds; ISM : individual (IC 348, NGC 1333); ISM : jets and outflows; stars : formation; stars : pre-main-sequence ID YOUNG STELLAR OBJECTS; MULTIBAND IMAGING PHOTOMETER; MOLECULAR CLOUD; STAR-FORMATION; CONTINUUM EMISSION; OUTFLOW SOURCES; CLUSTER IC-348; NGC 1333; PROTOSTARS; DUST AB We present observations of 10.6 deg(2) of the Perseus molecular cloud at 24, 70, and 160 mu m with Spitzer MIPS. The images show prominent, complex extended emission dominated by illuminating B stars on the east side of the cloud and by cold filaments of 160 mu m emission on the west side. Of 3950 point sources identified at 24 mu m, 1141 have 2MASS counterparts. A quarter of these populate regions of the K-s versus K-s - [24] diagram that are distinct from stellar photospheres and background galaxies and thus are likely to be cloud members with infrared excess. Nearly half ( 46%) of these 24 mu m excess sources are distributed outside the IC 348 and NGC 1333 clusters. A significant number of IRAS PSC objects are not recovered by Spitzer MIPS, most often because the IRAS objects were confused by bright nebulosity. The intercluster region contains several tightly clumped ( r similar to 0.1 pc) young stellar aggregates whose members exhibit a wide variety of infrared SEDs characteristic of different circumstellar environments. This could be explained by a significant age spread among the aggregate members, or if the members formed at the same time, a remarkably rapid circumstellar evolution would be required to account for the association of Class I and Class III sources at ages less than or similar to 1Myr. We highlight important results for the HH 211 flow, where the bow shocks are detected at both 24 and 70 mu m, and for the debris disk candidate BD + 31 643, where the MIPS data show the linear nebulosity to be an unrelated interstellar feature. Our data, mosaics, and catalogs are available at the Spitzer Science Archive for use by interested members of the community. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Natl Tsing Hua Univ, Astron Inst, Hsinchu 30043, Taiwan. Natl Tsing Hua Univ, Dept Phys, Hsinchu 30043, Taiwan. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Leiden Univ, NL-2300 RA Leiden, Netherlands. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70301 USA. RP Rebull, LM (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM luisa.rebull@jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012; OI Rebull, Luisa/0000-0001-6381-515X; Merin, Bruno/0000-0002-8555-3012 NR 80 TC 96 Z9 96 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2007 VL 171 IS 2 BP 447 EP 477 DI 10.1086/517607 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 199DO UT WOS:000248676600005 ER PT J AU Ruiterkamp, R Charnley, SB Butner, HM Huang, HC Rodgers, SD Kuan, YJ Ehrenfreund, P AF Ruiterkamp, R. Charnley, S. B. Butner, H. M. Huang, H.-C. Rodgers, S. D. Kuan, Y.-J. Ehrenfreund, P. TI Organic astrochemistry: observations of interstellar ketene SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE astrochemistry; ISM : abundances; ISM : clouds; ISM : molecules; stars; formation ID YOUNG STELLAR OBJECTS; GRAIN SURFACE-CHEMISTRY; MASSIVE STAR-FORMATION; MOLECULAR CLOUDS; IRAS 16293-2422; PROTOSTELLAR ENVIRONMENT; FORMALDEHYDE ORTHO; FORMING REGIONS; PARA RATIO; HOT CORES AB We have observed emission from both ortho and para spin states of ketene (CH2CO) towards several deeply-embedded protostars. The low CH2CO fractional abundances (similar to 10(-10)) and the rotation temperatures (similar to 20 K) are consistent with emission from the cooler envelope. We compare our results with previous studies and discuss possible production pathways to interstellar ketene. We suggest that, if low observed excitation temperatures of CH2CO, CH3CHO and H2CO are indicative of their absence from the hot core region, then this may be due to the extensive hydrogenation of pre-existing grain mantles prior to evaporation into the inner envelope, leading to lower abundances of these compounds and to mantles rich in alcohols. C1 NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. James Madison Univ, Dept Phys, Harrisonburg, VA 22807 USA. Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Leiden Univ, Leiden Inst Chem, NL-2300 RA Leiden, Netherlands. RP Charnley, SB (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM charnley@dusty.arc.nasa.gov RI Charnley, Steven/C-9538-2012; OI Butner, Harold/0000-0003-4899-2064 NR 57 TC 9 Z9 9 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD AUG PY 2007 VL 310 IS 3-4 BP 181 EP 188 DI 10.1007/s10509-007-9493-9 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 201EH UT WOS:000248813800002 ER PT J AU Dibb, JE Albert, M Courville, Z Anastasio, C Galbavy, ES Atlas, E Beyersdorf, AJ Blake, DR Meinardi, S Rowland, FS Swanson, AL Blake, NJ Bocquet, F Cohen, L Helmig, D Burkhart, JF Frey, MM Friel, DK Hutterli, MA Chen, G Conway, TJ Oltrnans, SJ AF Dibb, Jack E. Albert, Mary Courville, Zoe Anastasio, Cort Galbavy, Edward S. Atlas, Elliot Beyersdorf, Andreas J. Blake, Donald R. Meinardi, Simone Rowland, F. Sherwood Swanson, Aaron L. Blake, Nicola J. Bocquet, Florence Cohen, Lana Helmig, Detlev Burkhart, John F. Frey, Markus M. Friel, Donna K. Hutterli, Manuel A. Chen, Gao Conway, Thomas J. Oltrnans, Sairitiel J. TI An overview of air-snow exchange at Summit, Greenland: Recent experiments and findings SO ATMOSPHERIC ENVIRONMENT LA English DT Editorial Material ID SOUTH-POLE; NONMETHANE HYDROCARBONS; ISCAT 2000; OH; TROPOSPHERE; CHEMISTRY; H2SO4; HNO3; SINK; NOX C1 Univ New Hampshire, CCRC EOS, Durham, NH 03824 USA. Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. Univ Miami, Div Marine & Atomspher Chem, Coral Gables, FL 33124 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA. Univ Colorado, INSTAAR, Boulder, CO 80309 USA. Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. NASA Langley, Hampton, VA USA. NOAA, ESRL GMD, Washington, DC 20230 USA. RP Dibb, JE (reprint author), Univ New Hampshire, CCRC EOS, Morse Hall,39 Coll Rd, Durham, NH 03824 USA. EM jack.dibb@unh.edu RI Burkhart, John/B-7095-2008; Frey, Markus/G-1756-2012; Beyersdorf, Andreas/N-1247-2013; Atlas, Elliot/J-8171-2015; Steig, Eric/G-9088-2015; OI Burkhart, John/0000-0002-5587-1693; Frey, Markus/0000-0003-0535-0416; Steig, Eric/0000-0002-8191-5549; Lefer, Barry/0000-0001-9520-5495 NR 39 TC 13 Z9 13 U1 0 U2 13 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 AUG PY 2007 VL 41 IS 24 BP 4995 EP 5006 DI 10.1016/j.atmosenv.2006.12.006 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 203PL UT WOS:000248986400001 ER PT J AU Sjostedt, SJ Huey, LG Tanner, DJ Peischl, J Chen, G Dibb, JE Lefer, B Hutterli, MA Beyersdorf, AJ Blake, NJ Blake, DR Sueper, D Ryerson, T Burkhart, J Stohl, A AF Sjostedt, S. J. Huey, L. G. Tanner, D. J. Peischl, J. Chen, G. Dibb, J. E. Lefer, B. Hutterli, M. A. Beyersdorf, A. J. Blake, N. J. Blake, D. R. Sueper, D. Ryerson, T. Burkhart, J. Stohl, A. TI Observations of hydroxyl and the sum of peroxy radicals at Summit, Greenland during summer 2003 SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE HOx; Greenland; polar; photochemistry; hydroxyl radical; summit ID ABSORPTION CROSS-SECTIONS; PARTICLE DISPERSION MODEL; SOUTH-POLE; OZONE DESTRUCTION; HYDROGEN-PEROXIDE; INTERSTITIAL AIR; SURFACE SNOW; CHEMISTRY; OH; TROPOSPHERE AB The first measurements of peroxy (HO2 + RO2) and hydroxyl (OH) radicals above the arctic snowpack were collected during the summer 2003 campaign at Summit, Greenland. The median measured number densities for peroxy and hydroxyl radicals were 2.2 x 10(8) Mol cm(-3) and 6.4 x 10(6) mol cm(-3), respectively. The observed peroxy radical values are in excellent agreement (R-2 = 0.83, M/O = 1.06) with highly constrained model predictions. However, calculated hydroxyl number densities are consistently more than a factor of 2 lower than the observed values. These results indicate that our current understanding of radical sources and sinks is in accord with our observations in this environment but that there may be a mechanism that is perturbing the (HO2 + RO2)/OH ratio. This observed ratio was also found to depend on meteorological conditions especially during periods of high winds accompanied by blowing snow. Backward transport model simulations indicate that these periods of high winds were characterized by rapid transport (1-2 days) of marine boundary layer air to Summit. These data suggest that the boundary layer photochemistry at Summit may be periodically impacted by halogens. (C) 2007 Published by Elsevier Ltd. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. Univ Houston, Dept Geosci, Houston, TX 77204 USA. Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. British Antarctic Survey, Div Phys Sci, Cambridge CB3 0ET, England. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. NOAA, Aeron Lab, Boulder, CO 80305 USA. Unicv Calif Merced, Sch Engn, Merced, CA 95344 USA. Norwegian Inst Air Res, N-2027 Kjeller, Norway. RP Huey, LG (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM greg.huey@eas.gatech.edu RI Stohl, Andreas/A-7535-2008; Peischl, Jeff/E-7454-2010; Ryerson, Tom/C-9611-2009; Beyersdorf, Andreas/N-1247-2013; Sjostedt, Steven/B-5032-2015; Lefer, Barry/B-5417-2012; OI Stohl, Andreas/0000-0002-2524-5755; Peischl, Jeff/0000-0002-9320-7101; Lefer, Barry/0000-0001-9520-5495; Burkhart, John/0000-0002-5587-1693 NR 52 TC 59 Z9 61 U1 0 U2 25 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 AUG PY 2007 VL 41 IS 24 BP 5122 EP 5137 DI 10.1016/j.atmosenv.2006.06.065 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 203PL UT WOS:000248986400011 ER PT J AU Robinson, ML Baumgartner, ET Nickels, KM Litwin, TE AF Robinson, Matthew L. Baumgartner, Eric T. Nickels, Kevin M. Litwin, Todd E. TI Hybrid image plane/stereo (HIPS) manipulation for robotic space applications SO AUTONOMOUS ROBOTS LA English DT Article DE vision-based manipulation; stereo triangulation; stereo vision; space robotics AB Manipulation systems for planetary exploration operate under severe limitations due to power and weight restrictions and extreme environmental conditions. Typically such systems employ carefully calibrated stereo cameras and carefully calibrated manipulators to achieve precision on the order of ten millimeters with respect to instrument placement activities. The environmental and functional restrictions under which these systems are used limit the operational accuracy of these approaches. This paper presents a novel approach to stereo-based manipulation designed to robustly achieve high precision levels despite the aforementioned limitations. The basic principle of the approach, known as Hybrid Image Plane/Stereo (HIPS) Manipulation, is the generation of camera models through direct visual sensing of the manipulator's end-effector. The HIPS method estimates and subsequently uses these models to position the manipulator at a target location specified in the image-planes of a stereo camera pair using stereo correlation and triangulation. In-situ estimation and adaptation of the manipulator/camera models in this method accounts for changes in the system configuration, thus ensuring consistent precision for the life of the mission. The end result is a increase in positioning precision by a factor of approximately two for a limited version of HIPS, and an order of magnitude increase in positioning precision for the full on-line version of HIPS. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Ohio No Univ, Ada, OH 45810 USA. Trinity Univ, San Antonio, TX 78212 USA. RP Robinson, ML (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Matthew.L.Robinson@jpl.nasa.gov NR 27 TC 4 Z9 4 U1 0 U2 2 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 AUG PY 2007 VL 23 IS 2 BP 83 EP 96 DI 10.1007/s10514-007-9032-0 PG 14 WC Computer Science, Artificial Intelligence; Robotics SC Computer Science; Robotics GA 202YH UT WOS:000248940300002 ER PT J AU Donlon, C Robinson, I Casey, KS Vazquez-Cuervo, J Armstrong, E Arino, O Gentemann, C May, D LeBorgne, P Piolle, J Barton, I Beggs, H Poulter, DJS Merchant, CJ Bingham, A Heinz, S Harris, A Wick, G Emery, B Minnett, P Evans, R Llewellyn-Jones, D Mutlow, C Reynolds, RW Kawamura, H Rayner, N AF Donlon, C. Robinson, I. Casey, K. S. Vazquez-Cuervo, J. Armstrong, E. Arino, O. Gentemann, C. May, D. LeBorgne, P. Piolle, J. Barton, I. Beggs, H. Poulter, D. J. S. Merchant, C. J. Bingham, A. Heinz, S. Harris, A. Wick, G. Emery, B. Minnett, P. Evans, R. Llewellyn-Jones, D. Mutlow, C. Reynolds, R. W. Kawamura, H. Rayner, N. TI The global ocean data assimilation experiment high-resolution sea surface temperature pilot project SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID SATELLITE MEASUREMENTS; CLIMATE RESEARCH; INTERPOLATION AB An international collaboration of operational and research agencies is producing a new generation of SSTs, combining satellite microwave and infrared data and in situ observations, for NWP, ocean forecasting, ecosystem applications, and climate research. C1 Univ Southampton, Natl Oceanography Ctr, Southampton, Hants, England. Natl Oceanog Data Ctr, NOAA, Silver Spring, MD USA. JPL, NASA, PO DAAC, Pasadena, CA USA. European Space Agcy, Frascati, Italy. Remote Syst, Santa Rosa, CA USA. NAVOCEANO, Stennis Space Ctr, Mississippi State, MS USA. Ctr Meteorol Spatiale, Lannion, France. IFREMER, Ctr Brest, CERSAT, F-29280 Brest, France. CSIRO Marine & Atmospher Res, Hobart, Tas, Australia. Australian Bureau Meteorol, Melbourne, Vic, Australia. Univ Edinburgh, Edinburgh, Midlothian, Scotland. GeoLogics, Hilo, HI USA. Univ Maryland, CICS, NOAA, College Pk, MD 20742 USA. ESRL, NOAA, Boulder, CO USA. Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. Univ Leicester, Leicester, Leics, England. Rutherford Appleton Lab, Chilton, England. NCDC, NOAA, Asheville, NC USA. Tohoku Univ, JAXA, Tohoku, Japan. RP Donlon, C (reprint author), GODAE SST Pilot Project Office, Exeter EX1 3PB, Devon, England. EM craig.donlon@metoffice.gov.uk RI Casey, Kenneth/D-4065-2013; Merchant, Christopher/E-1180-2014 OI Casey, Kenneth/0000-0002-6052-7117; Merchant, Christopher/0000-0003-4687-9850 NR 18 TC 151 Z9 158 U1 3 U2 20 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD AUG PY 2007 VL 88 IS 8 BP 1197 EP 1213 DI 10.1175/BAMS-88-8-1197 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 205LA UT WOS:000249113800014 ER PT J AU Tao, WK Houze, R Smith, EA AF Tao, Wei-Kuo Houze, Robert, Jr. Smith, Eric A. TI The fourth TRMM latent heating workshop SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Washington, Seattle, WA 98195 USA. RP Tao, WK (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613 1, Greenbelt, MD 20771 USA. EM tao@agnes.gsfc.nasa.gov NR 1 TC 8 Z9 8 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD AUG PY 2007 VL 88 IS 8 BP 1255 EP 1259 DI 10.1175/BAMS-88-8-1255 PG 5 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 205LA UT WOS:000249113800019 ER PT J AU Kohler, MD Heaton, TH Bradford, SC AF Kohler, Monica D. Heaton, Thomas H. Bradford, Samuel C. TI Propagating waves in the steel, moment-frame factor building recorded during earthquakes SO BULLETIN OF THE SEISMOLOGICAL SOCIETY OF AMERICA LA English DT Article ID GROUND MOTIONS AB Wave-propagation effects can be useful in determining the system identification of buildings such as the densely instrumented University of California, Los Angeles, Factor building. Waveform data from the 72-channel array in the 17-story moment-resisting steel frame Factor building are used in comparison with finite-element calculations for predictive behavior. The high dynamic range of the 24-bit digitizers allows both strong motions and ambient vibrations to be recorded with reasonable signal-to-noise ratios. A three-dimensional model of the Factor building has been developed based on structural drawings. Observed displacements for 20 small and moderate, local and regional earthquakes were used to compute the impulse response functions of the building by deconvolving the subbasement records as representative input motions at its base. The impulse response functions were then stacked to bring out wave-propagation effects more clearly. The stacked data are used as input into theoretical dynamic analysis simulations of the building's response. C1 Univ Calif Los Angeles, Ctr Embedded Networked Sensing, Los Angeles, CA 90095 USA. CALTECH, Dept Civil Engn, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kohler, MD (reprint author), Univ Calif Los Angeles, Ctr Embedded Networked Sensing, Los Angeles, CA 90095 USA. NR 15 TC 56 Z9 60 U1 0 U2 3 PU SEISMOLOGICAL SOC AMER PI EL CERRITO PA PLAZA PROFESSIONAL BLDG, SUITE 201, EL CERRITO, CA 94530 USA SN 0037-1106 J9 B SEISMOL SOC AM JI Bull. Seismol. Soc. Amer. PD AUG PY 2007 VL 97 IS 4 BP 1334 EP 1345 DI 10.1785/0120060148 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 196SI UT WOS:000248501900022 ER PT J AU Nightingale, JM Hill, MJ Phinn, SR Held, AA AF Nightingale, J. M. Hill, M. J. Phinn, S. R. Held, A. A. TI Comparison of satellite-derived estimates of gross primary production for Australian old-growth tropical rainforest SO CANADIAN JOURNAL OF REMOTE SENSING LA English DT Article ID LIGHT-USE EFFICIENCY; NET PRIMARY PRODUCTION; PHOTOCHEMICAL REFLECTANCE INDEX; TERRESTRIAL PRIMARY PRODUCTION; RADIATION-USE EFFICIENCY; PRIMARY PRODUCTION GPP; PROCESS MODEL; SOUTHWESTERN OREGON; DECIDUOUS FOREST; CARBON BALANCE AB The moderate-resolution spectroradiometer (MODIS) sensor has provided estimates of near-real-time gross and annual net primary production (GPP and NPP) since March 2000. We compare 2 years (2000 and 2001) of satellite-based calculations of GPP in the seasonally wet tropical rainforests of north Queensland, Australia, with estimates derived from an ecosystem process model, physiological principles predicting growth using satellite data (3-PGS), that was previously calibrated with ground-based measurements at 21 sites. This comparison provides an independent evaluation of the MOD-17 GPP product because the 3-PGS simulations account for spatial variation in soil properties (available soil water and fertility) and rely on different sources of meteorological data and derived estimates of the fraction of photosynthetically active radiation (fPAR). Results of the comparison show that estimates of averaged annual and monthly GPP from MOD-17 are slightly higher in magnitude than those from 3-PGS, although the two models exhibit comparable seasonal dynamics over the 2-year analysis period. Some of the differences in estimates of productivity and temporal dynamics between 3-PGS and MODIS are a result of limitations in the types of input data used for each model. In addition, the particularly infertile soils of northern Australia account for a reduction in productivity that is not directly incorporated in the MOD-17 algorithm. Further testing and continued improvement of the MOD-17 input datasets and algorithm construction will see improved estimates of satellite-derived productivity in tropical forest regions across the globe. C1 Univ Queensland, Sch Geog Planning & Architect, Ctr Remote Sensing & Spatial Informat Sci, Biophys Remote Sensing Grp, Brisbane, Qld 4072, Australia. Australian Natl Univ, Cooperat Res Ctr Greenhouse Accounting, Canberra, ACT 2061, Australia. Univ N Dakota, Ctr Aerosp Sci, Grand Forks, ND 58202 USA. RP Nightingale, JM (reprint author), NASA, Goddard Space Flight Ctr, Terrestial Informat Syst Branch, Code 6145,Bld 32, Greenbelt, MD 20771 USA. EM jnight@ltpmail.gsfc.nasa.gov RI Held, Andre/A-4672-2011; OI Hill, Michael/0000-0003-4570-7467; Phinn, Stuart/0000-0002-2605-6104 NR 51 TC 1 Z9 1 U1 0 U2 10 PU CANADIAN AERONAUTICS SPACE INST PI KANATA PA 350 TERRY FOX DR, STE 104, KANATA, ON K2K 2W5, CANADA SN 1712-7971 J9 CAN J REMOTE SENS JI Can. J. Remote Sens. PD AUG PY 2007 VL 33 IS 4 BP 278 EP 288 PG 11 WC Remote Sensing SC Remote Sensing GA 209PO UT WOS:000249400700005 ER PT J AU Williams, KD Tselioudis, G AF Williams, K. D. Tselioudis, G. TI GCM intercomparison of global cloud regimes: present-day evaluation and climate change response SO CLIMATE DYNAMICS LA English DT Article ID SEA-SURFACE TEMPERATURE; HADLEY-CENTER; FEEDBACK PROCESSES; TROPICAL CLOUD; MODEL HADGEM1; CIRCULATION; SENSITIVITY; ATMOSPHERE; SIMULATIONS; VARIABILITY AB The radiative feedback from clouds remains the largest source of variation in climate sensitivity amongst general circulation models (GCMs). A cloud clustering methodology is applied to six contemporary GCMs in order to provide a detailed intercomparison and evaluation of the simulated cloud regimes. By analysing GCMs in the context of cloud regimes, processes related to particular cloud types are more likely to be evaluated. In this paper, the mean properties of the global cloud regimes are evaluated, and the cloud response to climate change is analysed in the cloud-regime framework. Most of the GCMs are able to simulate the principal cloud regimes, however none of the models analysed have a good representation of trade cumulus in the tropics. The models also share a difficulty in simulating those regimes with cloud tops at mid-levels, with only ECHAM5 producing a regime of tropical cumulus congestus. Optically thick, high top cloud in the extra-tropics, typically associated with the passage of frontal systems, is simulated considerably too frequently in the ECHAM5 model. This appears to be a result of the cloud type persisting in the model after the meteorological conditions associated with frontal systems have ceased. The simulation of stratocumulus in the MIROC GCMs is too extensive, resulting in the tropics being too reflective. Most of the global-mean cloud response to doubled CO2 in the GCMs is found to be a result of changes in the cloud radiative properties of the regimes, rather than changes in the relative frequency of occurrence (RFO) of the regimes. Most of the variance in the global cloud response between the GCMs arises from differences in the radiative response of frontal cloud in the extra-tropics and from stratocumulus cloud in the tropics. This variance is largely the result of excessively high RFOs of specific regimes in particular GCMs. It is shown here that evaluation and subsequent improvement in the simulation of the present-day regime properties has the potential to reduce the variance of the global cloud response, and hence climate sensitivity, amongst GCMs. For the ensemble of models considered in this study, the use of observations of the mean present-day cloud regimes suggests a potential reduction in the range of climate sensitivity of almost a third. C1 Hadley Ctr, Exeter EX1 3PB, Devon, England. Univ Reading, Environm Syst Sci Ctr, Exeter EX1 3PB, Devon, England. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Dept Appl Phys, New York, NY 10027 USA. RP Williams, KD (reprint author), Hadley Ctr, Met Off,FitzRoy Rd, Exeter EX1 3PB, Devon, England. EM keith.williams@metoffice.gov.uk NR 43 TC 78 Z9 79 U1 0 U2 20 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD AUG PY 2007 VL 29 IS 2-3 BP 231 EP 250 DI 10.1007/s00382-007-0232-2 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 178EI UT WOS:000247203600007 ER PT J AU Stothers, RB AF Stothers, Richard B. TI Three centuries of observation of stratospheric transparency SO CLIMATIC CHANGE LA English DT Article ID OPTICAL DEPTH PERTURBATIONS; LUNAR ECLIPSE COLORS; GREENLAND ICE CORE; VOLCANIC-ERUPTIONS; EXPLOSIVE VOLCANISM; CLIMATE; AEROSOLS; IMPACT; RECORD; PERIOD AB A chronology of stratospheric aerosol optical depth for the period 1671-1881 is derived from total lunar eclipse colors. It is compared with available proxy time series for the same period and with more refined data for more recent years. Contrary to previous speculations, the stratosphere from 1671 to 1881 seems to have been mostly undisturbed volcanically, with only two or three eruptions having injected into it truly significant amounts of aerosol-producing and climate-altering sulfur gases. It is confirmed that the full record for 1671-2000 shows a marked, though possibly quasiregular, similar to 80 year periodicity in stratospheric aerosol optical depth, which appears also in polar ice-core acidity records and in volcanic eruption frequencies. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Stothers, RB (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM rstothers@giss.nasa.gov NR 37 TC 3 Z9 3 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 J9 CLIMATIC CHANGE JI Clim. Change PD AUG PY 2007 VL 83 IS 4 BP 515 EP 521 DI 10.1007/s10584-007-9238-3 PG 7 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 189FC UT WOS:000247973800006 ER PT J AU Miller, S Papadopoulos, D Heimann, P Inghram, L McCorkle, L AF Miller, Sandi Papadopoulos, Demetrios Heimann, Paula Inghram, Linda McCorkle, Linda TI Graphite sheet coating for improved thermal oxidative stability of carbon fiber reinforced/PMR-15 composites SO COMPOSITES SCIENCE AND TECHNOLOGY LA English DT Article DE A. polymer matrix composites; B. high temperature properties; A. coating; A. hybrid compounds ID BARRIER PROPERTIES; SILICATE NANOCOMPOSITES; STABLE POLYIMIDES; DEGRADATION; TEMPERATURE; POLYMER AB Expanded graphite was compressed into graphite sheets and used as a coating for carbon fiber reinforced PMR-15 composites. BET analysis of the graphite indicated an increase in graphite pore size on compression, however the material was proven to be an effective barrier to oxygen when prepreged with PMR-15 resin. Oxygen permeability of the PMR-15/graphite was an order of magnitude lower than the compressed graphite sheet. By providing a barrier to oxygen permeation, the rate of oxidative degradation of PMR-15 resin was decreased. As a result, the composite thermo-oxidative stability increased by up to 25%. The addition of a graphite sheet as a top ply on the composites yielded little change in the material's flexural strength or interlaminar shear strength. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Polymers Branch, Cleveland, OH 44135 USA. Univ Akron, Dept Polymer Sci, Akron, OH 44325 USA. Ohio Aerosp Inst, Cleveland, OH USA. RP Miller, S (reprint author), NASA, Glenn Res Ctr, Polymers Branch, 2100 Brookpk Rd,MS 49-3, Cleveland, OH 44135 USA. EM Sandi.G.Miller@grc.nasa.gov NR 27 TC 3 Z9 3 U1 2 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0266-3538 J9 COMPOS SCI TECHNOL JI Compos. Sci. Technol. PD AUG PY 2007 VL 67 IS 10 BP 2183 EP 2190 DI 10.1016/j.compscitech.2005.10.022 PG 8 WC Materials Science, Composites SC Materials Science GA 183FH UT WOS:000247557600020 ER PT J AU Brewer, R AF Brewer, Ron TI EMC design for Wiringr and cabling SO EE-EVALUATION ENGINEERING LA English DT Article RP Brewer, R (reprint author), NASA, Kennedy Space Ctr, 300 E St SW, Washington, DC 20546 USA. EM ronbrewer@ieee.org NR 0 TC 0 Z9 0 U1 0 U2 0 PU NELSON PUBLISHING PI NOKOMIS PA 2500 NORTH TAMIAMI TRAIL, NOKOMIS, FL 34275-3482 USA SN 0149-0370 J9 EE-EVAL ENG JI EE-Eval. Eng. PD AUG PY 2007 VL 46 IS 8 BP 52 EP + PG 6 WC Engineering, Electrical & Electronic SC Engineering GA 197MZ UT WOS:000248561200009 ER PT J AU Binicioglu, S Can, MA Kiyachko, AA Shumovsky, AS AF Binicioglu, Sinem Can, M. Ali Kiyachko, Alexander A. Shumovsky, Alexander S. TI Entanglement of a single spin-1 object: An example of ubiquitous entanglement SO FOUNDATIONS OF PHYSICS LA English DT Article DE entanglement; quantum measurements; nonlocality ID QUANTUM-MECHANICS; MULTIPARTICLE ENTANGLEMENT; INFORMATION; STATES; ENTROPY; INEQUALITIES; NONLOCALITY; SYSTEMS; PHOTON AB Using a single spon-1 object as an example, we discuss a recent approach to quantum entanglement. [A.A. Klyachko and A.S. Shumovsky. J. Phys: Conf. Series 36. 87 (2006). E-print quant-phl051223]. The key idea of the approach consists in presetting of basic observables in the very definition of quantum system. Specification of basic observables defines the dynamic symmetry of the system. Entangled states of the system are then interpreted as states with maximal amount of uncertainty of all basic observables. The approach gives purely physical picture of entanglement. In particular, it separates principle physical properties of entanglement from inessential. Within the model example under consideration, we show relativiy of entanglement with respect to dynamic symmetry and argue exixtence of single-particle entanglement. A number of physical examples are considered. C1 Bilkent Univ, Dept Phys, TR-06800 Ankara, Turkey. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Bilkent Univ, Dept Math, TR-06800 Ankara, Turkey. RP Binicioglu, S (reprint author), Bilkent Univ, Dept Phys, TR-06800 Ankara, Turkey. EM sinem@fen.bilkent.edu.tr NR 90 TC 2 Z9 2 U1 2 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0015-9018 J9 FOUND PHYS JI Found. Phys. PD AUG PY 2007 VL 37 IS 8 BP 1253 EP 1277 DI 10.1007/s10701-007-9149-1 PG 25 WC Physics, Multidisciplinary SC Physics GA 207ZH UT WOS:000249289100005 ER PT J AU Adachi, T Kletetschka, G AF Adachi, Tomoko Kletetschka, Gunther TI Using oxygen isotope and magnetism to reconstruct the paleotemperature framework of ancient travertine deposits in Death Valley, CA SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Acad Sci Czech Republic, Inst Geol, Prague, Czech Republic. EM tomoko.adachi@gsfc.nasa.gov; kletetschka@gli.cas.cz RI Kletetschka, Gunther/C-9996-2011 OI Kletetschka, Gunther/0000-0002-0645-9037 NR 0 TC 0 Z9 0 U1 2 U2 9 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 AUG PY 2007 VL 71 IS 15 SU S BP A5 EP A5 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900027 ER PT J AU Amundson, R Ewing, SA Michalski, G Thiemens, M Kendall, C Nishiizumi, K McKay, C Chong, G AF Amundson, R. Ewing, S. A. Michalski, G. Thiemens, M. Kendall, C. Nishiizumi, K. McKay, C. Chong, G. TI The climatic and biotic thresholds on soil elemental cycling along an and to hyperarid rainfall gradient SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ Calif Berkeley, Berkeley, CA 94720 USA. Purdue Univ, W Lafayette, IN 47907 USA. Univ Calif San Diego, La Jolla, CA 92093 USA. US Geol Survey, Menlo Pk, CA 94025 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Catholica Norte, Antofagasta, Chile. EM earthy@nature.berkeley.edu NR 0 TC 2 Z9 2 U1 0 U2 4 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 AUG PY 2007 VL 71 IS 15 SU S BP A22 EP A22 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900058 ER PT J AU Becker, H Brandon, AD Walker, RJ AF Becker, H. Brandon, A. D. Walker, R. J. TI Geochemical tracing of core-mantle interaction: High-precision W isotopic data on komatiites using TIMS SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Lunar & Planetary Inst, Houston, TX 77058 USA. Free Univ Berlin, Inst Geol Wissensch, D-1000 Berlin, Germany. NASA, Lyndon B Johnson Space Ctr, ARES Div, Houston, TX 77058 USA. Univ Maryland, Dept Geol, College Pk, MD 20742 USA. EM hbecker@zedat.fu-berlin.de; alan.d.brandon@nasa.gov; rjwalker@geol.umd.edu 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A71 EP A71 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900156 ER PT J AU Bell, MS AF Bell, M. S. TI Experimental shock decomposition of siderite and the origin of magnetite in Martian Meteorite ALH84001 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ Houston, Dept Geosci, Houston, TX 77204 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM mary.sue.bell1@jsc.nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 1 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 AUG PY 2007 VL 71 IS 15 SU S BP A75 EP A75 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900165 ER PT J AU Bennett, V Brandon, A Heiss, J Nutman, A AF Bennett, V. Brandon, A. Heiss, J. Nutman, A. TI Crust-mantle dynamics in the early Earth: The (142-143) Nd and Hf-176 isotopic perspective SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia. NASA, Lyndon B Johnson Space Ctr, Houston, TX USA. Chinese Acad Geol Sci, Beijing, Peoples R China. EM vickie.bennett@anu.edu.au NR 2 TC 2 Z9 2 U1 0 U2 0 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 AUG PY 2007 VL 71 IS 15 SU S BP A79 EP A79 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900173 ER PT J AU Brandon, AD Graham, DW Waight, T Gautason, B AF Brandon, Alan D. Graham, David W. Waight, Tod Gautason, Bjarni TI Os-He isotope systematics of Iceland picrites: Evidence for a deep origin of the Iceland plume SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. Inst Geol, DK-1350 Copenhagen, Denmark. Univ Akureyri, Orkustofnun, IS-602 Akureyri, Iceland. EM alan.d.brandon@nasa.gov RI Waight, Tod/A-8262-2010 OI Waight, Tod/0000-0003-2601-1202 NR 0 TC 2 Z9 2 U1 0 U2 1 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 AUG PY 2007 VL 71 IS 15 SU S BP A119 EP A119 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900252 ER PT J AU Catling, DC Claire, MW Zahnle, KJ AF Catling, D. C. Claire, M. W. Zahnle, K. J. TI Archean methane, oxygen and sulfur SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. Univ Washington, Dept Astron, Astrobiol Program, Seattle, WA 98195 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM David.Catling@bristol.ac.uk RI Catling, David/D-2082-2009 NR 2 TC 0 Z9 0 U1 1 U2 3 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 AUG PY 2007 VL 71 IS 15 SU S BP A151 EP A151 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900315 ER PT J AU Claire, MW Catling, DC Zahnle, KJ AF Claire, M. W. Catling, D. C. Zahnle, K. J. TI Sulfate, methane, and the rise in atmospheric oxygen SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ Washington, Dept Astron, Astrobiol Program, Seattle, WA 98195 USA. Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM mclaire@astro.washington.edu; David.Catling@bristol.ac.uk; Kevin.J.Zahnle@nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 3 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 AUG PY 2007 VL 71 IS 15 SU S BP A176 EP A176 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900365 ER PT J AU Clemett, SJ Nakuma-Messenger, K Mckay, DS Sandford, SA AF Clemett, Simon J. Nakuma-Messenger, Keiko McKay, David S. Sandford, Scott A. TI Identification of aromatic organic matter from comet 81P/Wild 2 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 ERC Inc, NASA, JSC, Houston, TX 77058 USA. NASA, JSC, Houston, TX 77058 USA. NASA, Moffett Field, CA 94305 USA. EM simon.j.clemett@jsc.nasa.gov; keiko.nakamura-1@jsc.nasa.gov; david.s.mckay@jsc.nasa.gov; ssandford@maii.arc.nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A178 EP A178 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900369 ER PT J AU Coustenis, A Jennings, D Jolly, A Benilan, Y Vinatier, S Gautier, D Nixon, C Flasar, M Bjoraker, G Romani, P Royer, E AF Coustenis, A. Jennings, D. Jolly, A. Benilan, Y. Vinatier, S. Gautier, D. Nixon, C. Flasar, M. Bjoraker, G. Romani, P. Royer, E. TI Titan's current and future exploration SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Observ Paris, LESIA, F-92195 Meudon, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Paris 07, LISA, Paris, France. EM athena.coustenis@obspm.fr; Donald.E.Jennings@nasa.gov; jolly@lisa.univ-paris12.fr; benilan@lisa.univ-paris12.fr; sandrine.vinatier@obspm.fr; daniel.gautier@obspm.fr; conor.nixon@ssedmail.gsfc.nasa.gov; f.m.flasar@nasa.gov; gordon.l.bjoraker@nasa.gov; paul.n.romani@nasa.gov; emilie.royer@obspm.fr RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Romani, Paul/D-2729-2012; Bjoraker, Gordon/D-5032-2012 OI Nixon, Conor/0000-0001-9540-9121; NR 7 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A192 EP A192 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900397 ER PT J AU Danielson, LR Righter, K Leinenweber, K Wang, Y AF Danielson, L. R. Righter, K. Leinenweber, K. Wang, Y. TI In situ high P-T melting and phase equilibria experiments on the Allende meteorite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA. Argonne Natl Lab, APS, GSECARS, Argonne, IL 60439 USA. EM lisa.r.danielson@nasa.gov; kevin.righter-1@nasa.gov; kurtl@asu.edu; wang@cars.uchicago.edu NR 3 TC 0 Z9 0 U1 0 U2 1 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 AUG PY 2007 VL 71 IS 15 SU S BP A200 EP A200 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900412 ER PT J AU De Leuw, S Papanastassiou, DA Wasson, JT AF De Leuw, S. Papanastassiou, D. A. Wasson, J. T. TI Search for Cr isotopic anomalies in unequilibrated carbonaceous chondrites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY ID CHROMIUM C1 Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA USA. Jet Propuls Lab, Sci Div, Pasadena, CA USA. Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA USA. EM sdeleuw@ucia.edu NR 3 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A214 EP A214 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900441 ER PT J AU Debaille, V Yin, QZ Brandon, AD Jacobsen, B AF Debaille, V. Yin, Q.-Z. Brandon, A. D. Jacobsen, B. TI Lu-Hf and Sm-Nd isotopic study of Martian meteorites: Implications for early differentiation on Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Lunar & Planetary Inst, Houston, TX USA. Univ Calif Davis, Davis, CA 95616 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM debaille@lpi.usra.edu; yin@geology.ucdavis.edu; alan.d.brandon@nasa.gov; jacobsen@geology.ucdavis.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A208 EP A208 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900429 ER PT J AU Downes, H Mittlefehldt, DW AF Downes, H. Mittlefehldt, D. W. TI Processes in early planetesimals: evidence from ureilite meteorites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ London Birkbeck Coll, Sch Earth Sci, London WC1E 7HX, England. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM h.downes@ucl.ac.uk; david.w.mittlefehldt@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A235 EP A235 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789900483 ER PT J AU Kallmeyer, J D'Hondt, S AF Kallmeyer, Jens D'Hondt, Steven CA Knox-02RR Shipboard Sci Party TI Cell enumeration in extremely nutrient-poor sediments SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ Rhode Isl, Grad Sch Oceanog, NASA, Astrobiol Inst, Narragansett, RI 02882 USA. EM kallm@gfz-potsdam.de RI Kallmeyer, Jens/I-3554-2012 OI Kallmeyer, Jens/0000-0002-6440-1140 NR 0 TC 1 Z9 1 U1 0 U2 0 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 AUG PY 2007 VL 71 IS 15 SU S BP A460 EP A460 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901135 ER PT J AU Kletetschka, G Adachi, T Adamovic, J Mikula, V Chan, M AF Kletetschka, Gunther Adachi, Tomoko Adamovic, Jiri Mikula, Vilem Chan, Marjorie TI Utah and Czech Mars analog concretions; Aquatic hematite and goethite characterization SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. AS CR, Inst Geol, Prague, Czech Republic. Univ Utah, Salt Lake City, UT USA. EM kletetschka@gmail.gov; kletetschka@nasa.gov; kletetschka@gli.cas.cz; chan@earth.utah.edu RI Kletetschka, Gunther/C-9996-2011; Adamovic, Jiri/I-8754-2014 OI Kletetschka, Gunther/0000-0002-0645-9037; 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A493 EP A493 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901201 ER PT J AU Klingelhofer, G Morris, RN Rodionov, D Schroder, C Fleischer, I Yen, A Ming, D AF Klingelhoefer, G. Morris, R. N. Rodionov, D. Schroeder, C. Fleischer, Iris Yen, A. Ming, D. TI Jarosite and goethite identified by Mossbauer spectroscopy on the surface of Mars: Mineralogical evidence for aqueous processes SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY ID GUSEV CRATER C1 Univ Mainz, Inst Anorgan & Analyt Chem, D-55099 Mainz, Germany. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Space Res Inst IKI, Moscow, Russia. Jet Prop Lab, Pasadena, CA 91109 USA. EM klingel@mail.uni-mainz.de RI Schroder, Christian/B-3870-2009 OI Schroder, Christian/0000-0002-7935-6039 NR 5 TC 1 Z9 1 U1 0 U2 4 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 AUG PY 2007 VL 71 IS 15 SU S BP A494 EP A494 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901204 ER PT J AU Kraft, MD Sharp, TG Michalski, JR Rampe, EB AF Kraft, M. D. Sharp, T. G. Michalski, J. R. Rampe, E. B. TI Basalt weathering at high-latitude regions on Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY ID TES C1 Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM mdkraft@asu.edu; tsharp@asu.edu; jmichals@jpl.nasa.gov; liz.rampe@asu.edu NR 7 TC 1 Z9 1 U1 0 U2 0 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 AUG PY 2007 VL 71 IS 15 SU S BP A519 EP A519 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901253 ER PT J AU Messenger, S Nakamura-Messenger, K Keller, L Matrajt, G Clemett, S Ito, M AF Messenger, Scott Nakamura-Messenger, Keiko Keller, Lindsay Matrajt, Graciela Clemett, Simon Ito, Motoo TI Submicrometer organic grains: Widespread constituents of the early solar system SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY ID MATTER C1 NASA, Johnson Space Ctr, Robert M Walker Lab Space Sci, Houston, TX USA. ESCG, Jacobs Engn, Houston, TX 77058 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A657 EP A657 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901530 ER PT J AU Michalski, JR AF Michalski, Joseph R. TI Martian clay minerals: Context and implications for weathering of a basaltic crust SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY ID MARS C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Joseph.R.Michalski@jpl.nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A663 EP A663 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901541 ER PT J AU Ming, DW Clark, BC Morris, RV AF Ming, D. W. Clark, B. C. Morris, R. V. CA ATHENA SCI TEAM TI Crystal water on mars: Insights from the Mars Exploration Rovers SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 NASA, Johnson Space Ctr, Houston, TX 77058 USA. Lockheed Martin Space Syst, Denver, CO 80201 USA. EM douglas.w.ming@nasa.gov NR 4 TC 0 Z9 0 U1 1 U2 2 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 AUG PY 2007 VL 71 IS 15 SU S BP A670 EP A670 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901556 ER PT J AU Ming, DW AF Ming, Douglas W. TI Aqueous alteration of basalts: Earth, Moon, and Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 NASA, Johnson Space Ctr, ARES, Houston, TX 77058 USA. EM douglas.w.ming@nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A670 EP A670 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901555 ER PT J AU Nakamura-Messenger, K Zolensky, M AF Nakamura-Messenger, Keiko Zolensky, Michael CA Stardust Mineralogy Petrology TI The mineralogy of Comet Wild-2 nucleus samples - What we think we know and what we do not know SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. ESCG, Jacobs Engn, Houston, TX 77058 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A703 EP A703 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901621 ER PT J AU Ohmoto, H Watanabe, Y Allwood, A Burch, IW Knauth, LP Yamaguchi, KE Johnson, I Altinok, E AF Ohmoto, H. Watanabe, Y. Allwood, A. Burch, I. W. Knauth, L. P. Yamaguchi, K. E. Johnson, I. Altinok, E. TI Formation of probable lateritic soils similar to 3.43 Ga in the Pilbara Craton, western Australia SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Penn State Univ, Astrobiol Res Ctr, University Pk, PA 16802 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. NASA, Jet Propuls Lab, Pasadena, CA 91109 USA. Macquarie Univ, Dept Earth & Planetary Sci, N Ryde, NSW 2109, Australia. Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. JAMSTEC, IFREE, Kanagawa 2370061, Japan. EM ohmoto@geosc.psu.edu; aallwood@jpl.nasa.gov; Knauth@asu.edu; kosei@jamstec.go.jp; ijohnson@geosc.psu.edu; ealtinok@geose.psu.edu NR 0 TC 4 Z9 4 U1 0 U2 1 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 AUG PY 2007 VL 71 IS 15 SU S BP A733 EP A733 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901681 ER PT J AU Papineau, D Purohit, R Mehta, P Shirey, SB Fogel, ML AF Papineau, D. Purohit, R. Mehta, P. Shirey, S. B. Fogel, M. L. TI High primary productivity in stromatolitic phosphorites from the Paleoproterozoic Aravalli Supergroup SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Carnegie Inst Washington, Geophys Lab, Washington, DC 20005 USA. Carnegie Inst Washington, NASA Astrobiol Inst, Washington, DC 20005 USA. ML Sukhadia Univ, Dept Geol Sci, Udaipur, Rajasthan, India. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC USA. EM dpapineau@ciw.edu; ritesh_purohit@rediffmail.com; shirey@dtm.ciw.edu; m.fogel@gl.ciw.edu NR 0 TC 0 Z9 0 U1 0 U2 1 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 AUG PY 2007 VL 71 IS 15 SU S BP A751 EP A751 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901718 ER PT J AU Puchtel, IS Brandon, AD Walker, RJ Nisbet, EG AF Puchtel, I. S. Brandon, A. D. Walker, R. J. Nisbet, E. G. TI Pt-Re-Os isotope and HSE systematics of Belingwe komatiites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ Maryland, College Pk, MD 20740 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ London Royal Holloway & Bedford New Coll, Egham TW20 0EX, Surrey, England. EM ipuchtel@geol.umd.edu; alan.d.brandon@nasa.gov; walker@geol.umd.edu; e.nisbet@gl.rhul.ac.uk NR 0 TC 1 Z9 1 U1 0 U2 0 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 AUG PY 2007 VL 71 IS 15 SU S BP A812 EP A812 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789901840 ER PT J AU Slater, GF Brady, AL Laval, B Lim, DSS AF Slater, G. F. Brady, A. L. Laval, B. Lim, D. S. S. TI Constraining carbon sources and growth of microbialites in Pavilion Lake, BC using C-14 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada. Univ British Columbia, Dept Civil Engn, Vancouver, BC V5Z 1M9, Canada. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Laval, Bernard/J-9861-2012; Slater, Greg/B-5163-2013 OI Slater, Greg/0000-0001-7418-7566 NR 0 TC 0 Z9 0 U1 1 U2 2 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 AUG PY 2007 VL 71 IS 15 SU S BP A948 EP A948 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789902267 ER PT J AU Taylor, GJ Stopar, JD Hurowitz, JA McLennan, SM Boynton, WV Wyatt, MB Baloga, SM AF Taylor, G. J. Stopar, J. D. Hurowitz, J. A. McLennan, S. M. Boynton, W. V. Wyatt, M. B. Baloga, S. M. TI A view of Martian weathering from microns to hundreds of kilometers SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ Hawaii, Hawaii Inst Geophys, Honolulu, HI 96822 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Brown Univ, Providence, RI 02912 USA. Proxemy Res, Laytonville, MD 20882 USA. EM gjtaylor@higp.hawaii.edu RI Hurowitz, Joel/A-8862-2008 NR 0 TC 0 Z9 0 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A1007 EP A1007 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789902385 ER PT J AU Tielens, A AF Tielens, Alexander TI The origin and evolution of dust in the interstellar medium SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 NASA, Ames Res Ctr, Space Sci Div, Moffett Field, CA 94035 USA. EM atielens@mail.arc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2007 VL 71 IS 15 SU S BP A1021 EP A1021 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789902414 ER PT J AU Waight, T Brandon, AD Graham, DW Gautason, B AF Waight, Tod Brandon, Alan D. Graham, David W. Gautason, Bjarni TI Isotopic constraints on picritic magmatism, Iceland SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 17th Annual V M Goldschmidt Conference CY AUG, 2007 CL Cologne, GERMANY C1 Univ Copenhagen, Inst Geol & Geog, DK-1350 Copenhagen K, Denmark. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. Orkustofnun, IS-602 Akureyri, Iceland. Univ Akureyri, IS-602 Akureyri, Iceland. EM todw@geol.ku.dk RI Waight, Tod/A-8262-2010 OI Waight, Tod/0000-0003-2601-1202 NR 0 TC 0 Z9 0 U1 0 U2 1 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 AUG PY 2007 VL 71 IS 15 SU S BP A1078 EP A1078 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200VC UT WOS:000248789902528 ER PT J AU Michalski, JR Reynolds, SJ Niles, PB Sharp, TG Christensen, PR AF Michalski, Joseph R. Reynolds, Stephen J. Niles, Paul B. Sharp, Thomas G. Christensen, Philip R. TI Alteration mineralogy in detachment zones: Insights from Swansea, Arizona SO GEOSPHERE LA English DT Article DE detachment fault; K-metasomatism; infrared; emission spectroscopy; Arizona ID WEST-CENTRAL ARIZONA; POTASSIUM METASOMATISM; K-METASOMATISM; NEW-MEXICO; CALIFORNIA; MOUNTAINS; EXTENSION; TRANSPORT; FLUID; ROCKS AB Rocks in detachment zones are commonly enriched in K2O, thought to originate from K-metasomatism by basin brine associated with tectonically controlled basins in semiarid settings. We used infrared spectroscopic and remote sensing techniques to investigate the geologic and mineralogical context of K-metasomatism associated with the Buckskin-Rawhide detachment fault near Swansea, Arizona, where spectacular alteration and exceptional exposures are observed. The goals are to ( 1) determine the mineralogy associated with K2O enrichment in this area, ( 2) define the lithologic and structural controls on alteration in this region, and ( 3) construct a general model for alteration in detachments zones, context of K2O enrichment, and relation to detachment-related ore deposits. In the Swansea area, Miocene volcanic rocks were completely and pervasively altered in an early stage of K-metasomatism to ferruginous illite, K-feldspar, and hematite, and later replaced by calcite, celadonite, hematite, and jasper. The mineralogy of these altered rocks and their geologic context suggest initial K-metasomatism by warm, alkaline surface water and/or groundwater related to a Miocene lacustrine environment. We propose that the carbonate overprint occurred due to increased fluid temperatures as the K-metasomatized rocks moved down the detachment fault in an environment of high heat flow. The spatial distribution of alteration minerals observed in the field and from remote sensing data shows that alteration was driven by reactivity of host rocks and host-rock permeability; normal faults and fractures associated with detachment faulting were not significant conduits of hydrothermal fluids. These results illustrate well the spatial relationships between alteration minerals and fluid conduits in detachment zones, which are usually studied only by chemical analyses. C1 CALTECH, Jet Prop Lab, Geophys & Planetary Geosci Grp, Pasadena, CA 91109 USA. Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Michalski, JR (reprint author), CALTECH, Jet Prop Lab, Geophys & Planetary Geosci Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 34 TC 8 Z9 9 U1 0 U2 3 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 1553-040X J9 GEOSPHERE JI Geosphere PD AUG PY 2007 VL 3 IS 4 BP 184 EP 198 DI 10.1130/GES00080.1 PG 15 WC Geosciences, Multidisciplinary SC Geology GA 214FM UT WOS:000249721400001 ER PT J AU Schulze-Makuch, D Dohm, JM Fan, C Fairen, AG Rodriguez, JAP Baker, VR Finkg, W AF Schulze-Makuch, Dirk Dohm, James M. Fan, Chaojun Fairen, Alberto G. Rodriguez, J. A. P. Baker, Victor R. Finkg, Wolfgang TI Exploration of hydrothermal targets on Mars SO ICARUS LA English DT Review DE Mars; thermal histories; cratering; exobiology; astrobiology ID GROUND ICE INTERACTIONS; HAUGHTON IMPACT STRUCTURE; MASSIVE SULFIDE DEPOSITS; SMALL MARTIAN VALLEYS; IBERIAN PYRITE BELT; X-RAY SPECTROMETER; NEW-MEXICO; OMEGA/MARS EXPRESS; MERIDIANI-PLANUM; GEOTHERMAL SYSTEM AB Based on various lines of geologic, geomorphic, topographic, geophysical, spectral, and elemental evidence, we conclude that hydrothermal environments have certainly existed on Mars and are likely to still exist. Here, we present candidate targets of endogenic- and exogenic-driven hydrothermal environments on Mars based on a set of selection criteria and suggest strategies for the detection of such targets. This includes a re-evaluation of potential targets using both existing and yet-to-be-rel eased remote information provided by the instruments onboard the Mars orbiters and rovers. We also provide terrestrial analogs for possible martian hydrothermal environments to highlight the implications of these targets for potential martian life. This compilation and synthesis of data from martian localities indicating hydrothermal activity is timely and a first step towards prioritizing candidate targets for further investigation, which will likely add more targets to this list. Future in situ exploration will have to focus on the most promising of the hydrothermal targets and investigate them utilizing a novel integrated multi-tier, multi-agent reconnaissance mission architecture. (C) 2007 Elsevier Inc. All rights reserved. C1 Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. Univ Autonoma Madrid, CSIC, Ctr Biol Mol, E-28049 Madrid, Spain. Planetary Sci Inst, Tucson, AZ 85719 USA. CALTECH, Div Phys Math & Astron, Visual & Autonomous Explorat Syst Res Lab, Pasadena, CA 91125 USA. RP Schulze-Makuch, D (reprint author), Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. EM dirksm@wsu.edu RI Fan, Chaojun/A-9966-2010; Dohm, James/A-3831-2014; OI Schulze-Makuch, Dirk/0000-0002-1923-9746 NR 159 TC 48 Z9 50 U1 2 U2 15 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 AUG PY 2007 VL 189 IS 2 BP 308 EP 324 DI 10.1016/j.icarus.2007.02.007 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194AR UT WOS:000248316800002 ER PT J AU Moore, MH Hudson, RL Carlson, RW AF Moore, M. H. Hudson, R. L. Carlson, R. W. TI The radiolysis of SO2 and H2S in water ice: Implications for the icy jovian satellites SO ICARUS LA English DT Article DE ices; Jupiter; satellites; ices; IR spectroscopy; satellites; surfaces ID INFRARED MAPPING SPECTROMETER; OUTER SOLAR-SYSTEM; SULFURIC-ACID; GALILEAN SATELLITES; HYDROGEN-PEROXIDE; EUROPAS SURFACE; LOW-TEMPERATURES; OPTICAL-CONSTANTS; ION IRRADIATION; SPECTRA AB Spectra of Europa, Ganymede, and Callisto reveal surfaces dominated by frozen water, hydrated materials, and minor amounts of SO2, CO2, and H2O2. These icy moons undergo significant bombardment by jovian magnetospheric radiation (protons, electrons, and sulfur and oxygen ions) which alters their surface compositions. In order to understand radiation-induced changes on icy moons, we have measured the mid-infrared spectra of 0.8 MeV proton-irradiated SO2, H2S, and H2O-ice mixtures containing either SO2 or H2S. Samples with H2O/SO2 or H2O/H2S ratios in the 3-30 range have been irradiated at 86, 110, and 132 K, and the radiation half-lives Of SO2 and H2S have been determined. New radiation products include the H2S2 molecule and HSO3-, HSO4-, and SO42- ions, all with spectral features that make them candidates for future laboratory work and, perhaps, astronomical observations. Spectra of both unirradiated and irradiated ices have been recorded as a function of temperature, to examine thermal stability and phase changes. The formation of hydrated sulfuric acid in irradiated ice mixtures has been observed, along with the thermal evolution of hydrates to form pure sulfuric acid. These laboratory studies provide fundamental information on likely processes affecting the outer icy shells of Europa, Ganymede, and Callisto. Published by Elsevier Inc. C1 NASA, Goddard Space Flight Ctr, Astrochem Branch, Greenbelt, MD 20771 USA. Eckerd Coll, Dept Chem, St Petersburg, FL 33733 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Moore, MH (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Branch, Code 691, Greenbelt, MD 20771 USA. EM marla.h.moore@nasa.gov RI Hudson, Reggie/E-2335-2012 NR 66 TC 37 Z9 37 U1 0 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2007 VL 189 IS 2 BP 409 EP 423 DI 10.1016/j.icarus.2007.01.018 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194AR UT WOS:000248316800009 ER PT J AU Fletcher, LN Irwin, PGJ Teanby, NA Orton, GS Parrish, PD de Kok, R Howett, C Calcutt, SB Bowles, N Taylor, FW AF Fletcher, L. N. Irwin, P. G. J. Teanby, N. A. Orton, G. S. Parrish, P. D. de Kok, R. Howett, C. Calcutt, S. B. Bowles, N. Taylor, F. W. TI Characterising Saturn's vertical temperature structure from Cassini/CIRS SO ICARUS LA English DT Article DE Saturn; atmospheres; composition; atmospheres; structure ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; VOYAGER INFRARED MEASUREMENTS; HUBBLE-SPACE-TELESCOPE; PARA-HYDROGEN FRACTION; CLOUD STRUCTURE; OUTER PLANETS; EQUATORIAL REGION; UPPER TROPOSPHERE; THERMAL STRUCTURE; HELIUM ABUNDANCE AB Thermal infrared spectra of Saturn from 10-1400 cm(-1) at 15 cm(-1) spectral resolution and a spatial resolution of 1 degrees-2 degrees latitude have been obtained by the Cassini Composite Infrared Spectrometer [Flasar, F.M., and 44 colleagues, 2004. Space Sci. Rev. 115, 169-297]. Many thousands of spectra, acquired over eighteen-months of observations, are analysed using an optimal estimation retrieval code [Irwin, P.G.J., Parrish, P., Fouchet, T., Calcutt, S.B., Taylor, F.W., Simon-Miller, A.A., Nixon, C.A., 2004. Icarus 172, 37-49] to retrieve the temperature structure and para-hydrogen distribution over Saturn's northern (winter) and Southern (summer) hemispheres. The vertical temperature structure is analysed in detail to study seasonal asymmetries in the tropopause height (65-90 mbar), the location of the radiative-comective boundary (350-500 mbar), and the variation with latitude of a temperature knee (between 150 and 300 mbar) which was first observed in inversions of Voyager/IRIS spectra [Hanel, R., and 15 colleagues, 1981. Science 212, 192-200; Hanel, R., Conrath, B., Flasar, F.M., Kunde, V., Maguire, W., Pearl, J.C., Pirraglia, J., Samuelson, R., Cruikshank, D.P., Gautier, D., Gierasch, P.J., Horn, L., Ponnamperuma, C., 1982. Science 215, 544-548]. Uncertainties due to both the modelling of spectral absorptions (collision-induced absorption coefficients, tropospheric hazes, helium abundance) and the nature of our retrieval algorithm are quantified. Temperatures in the stratosphere near 1 mbar show a 25-30 K temperature difference between the north pole and south pole. This asymmetry becomes less pronounced with depth as the radiative time constant for the atmospheric response increases at deeper pressure levels. Hemispherically-symmetric small-scale temperature structures associated with zonal winds are superimposed onto the temperature asymmetry for pressures greater than 100 mbar. The para-hydro.-en fraction in the 100-400 mbar range is greater than equilibrium predictions for the southern hemisphere and parts of the northern hemisphere, and less than equilibrium predictions polewards of 40 degrees N. The temperature knee between 150-300 mbar is larger in the summer hemisphere than in the winter, smaller and higher at the equator, deeper and larger in the equatorial belts and small at the poles. Solar heating on tropospheric haze is proposed as a possible mechanism for this effect; the increased efficiency of ortho- to pora-hydrogen conversion in the southern hemisphere is consistent with the presence of larger aerosols in the Summer hemisphere, which we demonstrate to be qualitatively consistent with previous studies of Saturn's tropospheric aerosol distribution. (C) 2007 Elsevier Inc. All rights reserved. C1 Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fletcher, LN (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England. EM fletcher@atm.ox.ac.uk RI Fletcher, Leigh/D-6093-2011; OI Fletcher, Leigh/0000-0001-5834-9588; Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X NR 70 TC 50 Z9 50 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2007 VL 189 IS 2 BP 457 EP 478 DI 10.1016/j.icarus.2007.02.006 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194AR UT WOS:000248316800012 ER PT J AU Del Genio, AD Barbara, JM Ferrier, J Ingersoll, AP West, RA Vasavada, AR Spitale, J Porco, CC AF Del Genio, Anthony D. Barbara, John M. Ferrier, Joseph Ingersoll, Andrew P. West, Robert A. Vasavada, Ashwin R. Spitale, Joseph Porco, Carolyn C. TI Saturn eddy momentum fluxes and convection: First estimates from Cassini images SO ICARUS LA English DT Article DE Saturn; atmosphere; atmospheres; dynamics; meteorology; jovian planets ID 1990 EQUATORIAL DISTURBANCE; JUPITERS ATMOSPHERE; MOIST CONVECTION; IMAGING SCIENCE; ZONAL WINDS; CLOUD STRUCTURE; UPPER TROPOSPHERE; VOYAGER-1 IMAGES; GIANT PLANETS; EVOLUTION AB We apply an automated cloud feature tracking algorithm to estimate eddy momentum fluxes in Saturn's southern hemisphere from Cassini Imaging Science Subsystem near-infrared continuum image sequences. Voyager Saturn manually tracked images had suggested no conversion of eddy to mean flow kinetic energy, but this was based on a small sample of <1000 wind vectors. The automated procedure we use for the Cassini data produces an order of magnitude more usable wind vectors with relatively unbiased sampling. Automated tracking is successful in and around the westward jet latitudes on Saturn but not in the vicinity of most eastward jets, where the linearity and non-discrete nature of cloud features produces ambiguous results. For the regions we are able to track, we find peak eddy fluxes similar to 10 m(2) s(-2) and a clear positive correlation between eddy momentum fluxes and meridional shear of the mean zonal wind, implying that eddies supply momentum to eastward jets and remove momentum from westward jets at a rate similar to 5 x 10(-6) m s(-2). The behavior we observe is similar to that seen on Jupiter, though with smaller eddy-mean kinetic energy conversion rates per unit mass of atmosphere (3.3 x 10(-5) m(2) s(-3)). We also use the appearance and rapid evolution of small bright features at continuum wavelengths, in combination with evidence from weak methane band images where possible, to diagnose the occurrence of moist convective storms on Saturn. Areal expansion rates imply updraft speeds of similar to 1 m s(-1) over the convective anvil cloud area. As on Jupiter, convection preferentially occurs in cyclonic shear regions on Saturn, but unlike Jupiter, convection is also observed in eastward jet regions. With one possible exception, the large eddy fluxes seen in the cyclonic shear latitudes do not seem to be associated with convective events. (C) 2007 Elsevier Inc. All rights reserved. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Inst Space Studies, LLC, New York, NY 10025 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Space Sci Inst, Cassini Imaging Cent Lab Operat, Boulder, CO 80301 USA. RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM adelgenio@giss.nasa.gov RI Del Genio, Anthony/D-4663-2012 OI Del Genio, Anthony/0000-0001-7450-1359 NR 47 TC 33 Z9 33 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2007 VL 189 IS 2 BP 479 EP 492 DI 10.1016/j.icarus.2007.02.013 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194AR UT WOS:000248316800013 ER PT J AU Orton, GS Gustafsson, M Burgdorf, M Meadows, V AF Orton, Glenn S. Gustafsson, Magnus Burgdorf, Martin Meadows, Victoria TI Revised ab initio models for H-2-H-2 collision-induced absorption at low temperatures SO ICARUS LA English DT Article DE atmospheres, structure; Uranus; Neptune; infrared observations; spectroscopy ID HELIUM ABUNDANCE; SPECTRA; URANUS; PAIRS; NEPTUNE; BAND; GAS AB A revised ab initio calculation of the H-2-H-2 collision-induced absorption results in significant differences compared with the work of J. Borysow et al. [Borysow, J., Trafton, L., Frommhold, L., Birnbaum, G., 1985. Astrophys. J. 296, 644-654] for wavenumbers greater than 600 cm(-1) and temperatures below 120 K. The revision has significant influence on the spectra of Uranus and Neptune, and essentially removes the need for models with "super-solar" helium abundances or stratospheric hazes to explain the spectrum of Uranus. (C) 2007 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Orton, GS (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM go@orton.jpl.nasa.gov RI Gustafsson, Magnus/A-1661-2010 OI Gustafsson, Magnus/0000-0002-7629-0169 NR 16 TC 22 Z9 22 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2007 VL 189 IS 2 BP 544 EP 549 DI 10.1016/j.icarus.2007.02.003 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194AR UT WOS:000248316800017 ER PT J AU Milliken, RE Mustard, JF AF Milliken, Ralph E. Mustard, John F. TI Estimating the water content of hydrated minerals using reflectance spectroscopy. I. Effects of darkening agents and low-albedo materials SO ICARUS LA English DT Article DE spectroscopy; Mars, surface; infrared observations; asteroids, composition; mineralogy ID COMMON GEOLOGIC MINERALS; E-CLASS ASTEROIDS; CARBONACEOUS CHONDRITES; OMEGA/MARS EXPRESS; QUANTITATIVE-ANALYSIS; SPECTRAL REFLECTANCE; MU-M; MIXTURES; MARS; SPECTROMETER AB The apparent strength of absorptions due to H2O near 1.9 and 3 mu m in reflectance spectra is strongly affected by sample albedo. This study uses experimental and analytical approaches to quantify the effects of albedo on estimating the water content of hydrated minerals using various band parameters. We compare spectral band parameters for a series of low-albedo physical and numerical mixtures to measured water contents. Physical experiments consist of montmorillonite, clinoptilolite, and palagonite mixed with lesser amounts of carbon black and ilmenite, whereas numerical mixtures are composed of these host minerals mixed with a material of constant, low albedo. We find the effective single-particle absorption-thickness parameter provides the best correlation to water content, independent of composition and albedo, when derived from continuum-removed single scattering albedo spectra. Uncertainties in estimated water content are on the order of +/- 1 wt% using this method. The normalized optical path length parameter provides the best correlation to water content when using reflectance spectra, yielding estimates within +/- 1.6 wt% H2O. The accuracy of these models is related to the physical nature of the darkening material. Scattering and absorption efficiencies are easier to model for intimate mixtures containing relatively large, dark grains than mixtures dominated by coatings of a fine-grained, strongly absorbing material. This suggests the physical properties that give rise to the albedo of a material are an important factor for accurate estimates of absolute water content. (C) 2007 Elsevier Inc. All rights reserved. C1 Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RP Milliken, RE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ralph.milliken@jpl.nasa.gov NR 37 TC 31 Z9 31 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2007 VL 189 IS 2 BP 550 EP 573 DI 10.1016/j.icarus.2007.02.017 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194AR UT WOS:000248316800018 ER PT J AU Milliken, RE Mustard, JF AF Milliken, Ralph E. Mustard, John F. TI Estimating the water content of hydrated minerals using reflectance spectroscopy. II. Effects of particle size SO ICARUS LA English DT Article DE spectroscopy ID COMMON GEOLOGIC MINERALS; INFRARED REFLECTANCE; THERMAL INERTIA; QUANTITATIVE-ANALYSIS; SPECTRAL REFLECTANCE; HYDROUS MINERALS; MARTIAN SURFACE; GRAIN SIZES; MU-M; MARS AB Visible-near infrared reflectance spectra for five particle size fractions of a Hawaiian palagonite (HWMK101) and a nontronite (ferruginous smectite, Clay Minerals Society source clay SWa-l) were measured under ambient, purged, and heated conditions to characterize the effects of surface and volume scattering on the relationship between absolute H2O content and the strength of the 3 pm absorption feature. Both materials were ground and dry sieved to particle sizes of <25, 25-45, 45-75, 75-125, and 125-250 mu m. Particles of the bulk palagonite have an approximate bimodal distribution consisting of small, amorphous particles <5 mu m in diameter mixed with crystalline and glass particles <1 mm in diameter, whereas the nontronite particles are polycrystalline aggregates. We find that band parameters value relating the strength of the 3 mu m hydration feature to water content increase with particle size for a given water content, regardless of whether reflectance or single scattering albedo spectra are used. Spectra generally increase in reflectance as particle size decreases, a result of the relative increase in volume to surface scattering. Spectra of large particles are commonly saturated in the 3 mu m region due to an increase in optical path length, making an accurate estimate of water content indeterminate until the samples dehydrate to the volume-scattering regime. We find that the presence of fines in several of the size fractions of palagonite cause their spectra to be representative of the finest fraction rather than the mean particle size. The nontronite spectra appear to be representative of an effective particle size within the range of the sieved size fractions. Many planetary surfaces are expected to have a large number of small particles which can dominate their spectral signature. Our results for particles <45 mu m provide a reasonable model for estimating the H2O content of hydrated asteroids and regions of Mars. (C) 2007 Elsevier Inc. All rights reserved. C1 Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RP Milliken, RE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ralph.milliken@jpl.nasa.gov NR 43 TC 18 Z9 18 U1 1 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 J9 ICARUS JI Icarus PD AUG PY 2007 VL 189 IS 2 BP 574 EP 588 DI 10.1016/j.icarus.2006.12.028 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194AR UT WOS:000248316800019 ER PT J AU Lee, DU Kim, H Jones, CR Villasenor, JD AF Lee, Dong-U Kim, Hyungjin Jones, Christopher R. Villasenor, John D. TI Pilotless frame synchronization via LDPC code constraint feedback SO IEEE COMMUNICATIONS LETTERS LA English DT Article DE block codes; channel coding; frame synchronization ID OPTIMUM AB In traditional receiver architectures, frame synchronization is performed using pilot symbols and a correlation rule. In this paper we show that outputs from the constraint node side of a bipartite decoding graph can be used to achieve frame synchronization in a pilotless Low-Density Parity-Check (LDPC) coded transmission, thereby avoiding the bandwidth cost inherent in use of pilot symbols. The complexity of the frame synchronizer is kept relatively low due to its XOR-based approach. C1 Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lee, DU (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. EM dongu@icsl.ucla.edu; hjkimnov@ee.ucla.edu; christop@jpl.nasa.gov; villa@icsl.ucla.edu NR 5 TC 5 Z9 5 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1089-7798 J9 IEEE COMMUN LETT JI IEEE Commun. Lett. PD AUG PY 2007 VL 11 IS 8 BP 683 EP 685 DI 10.1109/LCOMM.2007.070525 PG 3 WC Telecommunications SC Telecommunications GA 196YW UT WOS:000248520600015 ER PT J AU Fu, FW Stoenescu, TM van der Schaar, M AF Fu, Fangwen Stoenescu, Tudor M. van der Schaar, Mihaela TI A Pricing Mechanism for Resource Allocation in Wireless Multimedia Applications SO IEEE JOURNAL OF SELECTED TOPICS IN SIGNAL PROCESSING LA English DT Article DE Game theory; multiuser wireless multimedia streaming; pricing mechanism; resource allocation ID TAIL PROBABILITIES; NETWORKS AB We consider the problem of multiuser resource allocation for wireless multimedia applications deployed by autonomous and noncollaborative wireless stations (WSTAs). Existing resource allocation solutions for WLANs are not network-aware and do not take into account the selfish behavior of individual WSTAs. Specifically, the selfish WSTAs can manipulate the network by untruthfully representing their private information (i.e., video characteristics, experienced channel conditions, and deployed streaming strategies). This often results in inefficient resource allocations. To overcome this obstacle, we present a pricing mechanism for message exchanges between the WSTAs and the Central Spectrum Moderator (CSM). The messages represent network-aware resource demands and corresponding prices. We prove that the message exchanges reach the Nash equilibrium and that the resulting equilibrium messages generate allocations which are efficient, budget balanced, and satisfy voluntary participation. The simulation results verify that these properties hold when the WSTAs behave strategically. Additionally, we evaluate the impact of initial prices and network congestion level on the convergence rate of message exchanges. C1 [Fu, Fangwen; van der Schaar, Mihaela] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. [Stoenescu, Tudor M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fu, FW (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. EM fwfu@ee.ucla.edu; tudor@caltech.edu; mihaela@ee.ucla.edu NR 39 TC 19 Z9 19 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1932-4553 J9 IEEE J-STSP JI IEEE J. Sel. Top. Signal Process. PD AUG PY 2007 VL 1 IS 2 BP 264 EP 279 DI 10.1109/JSTSP.2007.901519 PG 16 WC Engineering, Electrical & Electronic SC Engineering GA 437NS UT WOS:000265494800006 ER PT J AU Lin, YM Guo, JY Shapiro, AA Shi, FG AF Lin, Yaomin Guo, Jingyan Shapiro, Andrew A. Shi, Frank G. TI WIAD minimization in butterfly laser module packages: Clip design SO IEEE TRANSACTIONS ON ADVANCED PACKAGING LA English DT Article DE butterfly laser module packages; fiber-optic packaging; finite-element methods; laser welding; post-weld shift; welding-induced alignment distortion ID INDUCED-ALIGNMENT-DISTORTION; POST-WELD-SHIFT; SEQUENCE AB Welding-induced alignment distortion (WIAD) is a serious issue in photonics packaging using laser welding, which may significantly affect the packaging yield. An elimination or minimization of the WIAD in butterfly laser module packaging is possible if process parameters or laser parameters are optimized. This work reports the attempt in WIAD reduction by design of the packaging weld clip. Seven types of weld clips were designed and implemented in the butterfly laser module packaging process. The WIADs with different weld clips were analyzed by means of numerical simulations by the finite-element method. It was concluded that the weld clip design affects the WIAD through the weld pattern distribution, and that the distortion can be controlled within a minimal range by proper design of the weld clip and the laser welding sequence. C1 Univ Virginia, Natl Inst Aerosp, Hampton, VA 23666 USA. Newport Corp, Irvine, CA 92606 USA. CALTECH, Jet Prop Lab, Enterprise Engn Div, Pasadena, CA 91109 USA. Univ Calif Irvine, Irvine, CA 92697 USA. RP Lin, YM (reprint author), Univ Virginia, Natl Inst Aerosp, Hampton, VA 23666 USA. EM yaominl@virginia.edu; jingyan.guo@newport.com; andrew.a.shapiro@jpl.nasa.gov; fgshi@uci.edu OI Lin, Yaomin/0000-0002-6509-308X NR 16 TC 2 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 1521-3323 J9 IEEE T ADV PACKAGING JI IEEE Trans. Adv. Packag. PD AUG PY 2007 VL 30 IS 3 BP 499 EP 505 DI 10.1109/TADVP.2007.901528 PG 7 WC Engineering, Manufacturing; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 199BM UT WOS:000248671200019 ER PT J AU Smith, RS Hadaegh, FY AF Smith, Roy S. Hadaegh, Fred Y. TI Closed-loop dynamics of cooperative vehicle formations with parallel estimators and communication SO IEEE TRANSACTIONS ON AUTOMATIC CONTROL LA English DT Article DE cooperative control; decentralized control; decentralized estimation; formation control; multi-agent control ID DECENTRALIZED CONTROL; SYSTEMS; STABILITY; COORDINATION AB The control of cooperative formations of vehicles can be based on parallel estimation, where each vehicle determines its control action from a locally maintained estimate of the entire observable formation state. Vehicles may communicate with one another allowing the local estimates to incorporate information from other estimators in the formation. This paper studies the dynamics that arise in this situation and provides a complete analysis of the formation stability for this class of decentralized control problems. In the absence of communication, the local estimator-controllers' open-loop dynamics necessarily appear in the closed-loop system dynamics, giving a more stringent closed-loop stability condition than in the single controller case. The estimators achieve consensus if and only if the controllers' open-loop dynamics are stable. Communication amongst the estimators can be used to specify the complete system dynamics and we present a framework for the analysis and design of communicated information links in the formation. We relate the complete closed-loop system poles to the transmitter and receiver gains, and the spectral properties of the Laplacian of the graph describing the communication links within the formation. These results also apply to parallel estimation problems in other applications including power system control and redundant channel control architectures. C1 Univ Calif Santa Barbara, Dept Elect & Comp Engn, Santa Barbara, CA 93106 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Smith, RS (reprint author), Univ Calif Santa Barbara, Dept Elect & Comp Engn, Santa Barbara, CA 93106 USA. RI Smith, Roy/C-7340-2009 OI Smith, Roy/0000-0002-8139-4683 NR 53 TC 57 Z9 57 U1 0 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9286 EI 1558-2523 J9 IEEE T AUTOMAT CONTR JI IEEE Trans. Autom. Control PD AUG PY 2007 VL 52 IS 8 BP 1404 EP 1414 DI 10.1109/TAC.2007.902735 PG 11 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 200MK UT WOS:000248767300004 ER PT J AU Freeman, A AF Freeman, Anthony TI Fitting a two-component scattering model to polarimetric SAR data from forests SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE polarimetry; scattering mechanisms; synthetic aperture radar (SAR); tropical and temperate forests ID SYMMETRY PROPERTIES; RADAR POLARIMETRY; DECOMPOSITION; IMAGERY AB Two simple scattering mechanisms are fitted to polarimetric synthetic aperture radar (SAR) observations of forests. The mechanisms are canopy scatter from a reciprocal medium with azimuthal symmetry and a ground scatter term that can represent double-bounce scatter from a pair of orthogonal surfaces with different dielectric constants or Bragg scatter from a moderately rough surface, which is seen through a layer of vertically oriented scatterers. The model is shown to represent the behavior of polarimetric backscatter from a tropical forest and two temperate forest sites by applying it to data from the National Aeronautic and Space Agency/Jet Propulsion Laboratory's Airborne SAR (AIRSAR) system. Scattering contributions from the two basic scattering mechanisms are estimated for clusters (of pixels in polarimetric SAR images. The solution involves the estimation of four parameters from four separate equations. This model fit approach is justified as a simplification of more complicated scattering models, which require many inputs to solve the forward scattering problem. The model is used to develop an understanding of the ground-trunk double-bounce scattering that is present in the data, which is seen to vary considerably as a function of incidence angle. Two parameters in the model fit appear to exhibit sensitivity to vegetation canopy structure, which is worth further exploration. Results from the model fit for the ground scattering term are compared with estimates from a forward model and shown to be in good agreement. The behavior of I he scattering from the ground-trunk interaction is consistent with the presence of a pseudo-Brewster angle effect for the air-trunk scattering interface. If the Brewster angle is known, it is possible to directly estimate the real part of the dielectric constant of the trunks, a key variable in forward modeling of backscatter from forests. It is also shown how, with a priori knowledge of the forest height, an estimate for the attenuation coefficient of the canopy can be obtained directly from the multi-incidence-angle polarimetric (observations. This attenuation coefficient is another key variable in forward models and is generally related to the canopy density. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Freeman, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 26 TC 76 Z9 85 U1 3 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2007 VL 45 IS 8 BP 2583 EP 2592 DI 10.1109/TGRS.2007.897929 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 195NO UT WOS:000248419100019 ER PT J AU Moghaddam, M Rahmat-Samii, Y Rodriguez, E Entekhabi, D Hoffman, J Moller, D Pierce, LE Saatchi, S Thomson, M AF Moghaddam, Mahta Rahmat-Samii, Yahya Rodriguez, Ernesto Entekhabi, Dara Hoffman, James Moller, Delwyn Pierce, Leland E. Saatchi, Sassan Thomson, Mark TI Microwave observatory of subcanopy and subsurface (MOSS): A mission concept for global deep soil moisture observations SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE canopy penetrating radar; large-aperture antennas; radar remote sensing; soil moisture; subsurface radar ID ELECTROMAGNETIC SCATTERING; FARADAY-ROTATION; ROUGH SURFACES; FOREST BIOMASS; IMAGING RADARS; MODEL; BACKSCATTER; WATER AB The microwave observatory of subcanopy and subsurface (MOSS) is a mission concept for a spaceborne synthetic aperture radar (SAR) system that provides global observations of soil moisture under substantial vegetation cover (exceeding 20 kg/m(2)) and at useful depths (1-5 m). The concept was developed and a number of new required technologies were demonstrated through a National Aeronautics and Space Administration Earth Science Technology Office Instrument Incubator Program project. This very high frequency (VHF)/ultrahigh frequency (UHF) polarimetric SAR is designed to provide 1-10-day observations of soil moisture at 1-km resolution. The rapid repeat cycle mandates swath widths in the range of 300-400 km, which must be realized by a 30-m-long antenna. Conventional array implementations would result in a mass of more than 4000 kg, whereas With the technology proposed and demonstrated in this project, the total antenna mass is less than 500 kg. The antenna concept is a dual-stacked patch array feed illuminating a 30-m mesh reflector to synthesize the long apertures and achieve the wide swath. The feed system prototype was fabricated and its performance demonstrated. Other major project components were: 1) system-level SAR and mission design; 2) demonstration of science data and products, using a tower-based VHF/UHF radar; 3) spacecraft and mesh reflector antenna mechanical design; 4) developing mitigation strategies for ionospheric effects; and 5) assessing frequency interference effects. Experimental science data were generated from the tower radar for soil moisture profiling in Arizona and for forest penetration in Oregon. The soil moisture products were demonstrated through an integrated inversion-processing algorithm. This paper summarizes the results from the MOSS project and demonstrates the feasibility of the spaceborne mission. C1 Univ Michigan, Ann Arbor, MI 48109 USA. Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA USA. MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. Univ Michigan, Dept Elect Engn & Comp Sci, Radiat Lab, Ann Arbor, MI 48109 USA. RP Moghaddam, M (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA. NR 36 TC 20 Z9 21 U1 1 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2007 VL 45 IS 8 BP 2630 EP 2643 DI 10.1109/TGRS.2007.898236 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 195NO UT WOS:000248419100024 ER PT J AU D'Alimonte, D Zibordi, G Berthon, JF AF D'Alimonte, Davide Zibordi, Giuseppe Berthon, Jean-Francois TI A statistical index of bio-optical seawater types SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE ocean color; remote sensing; water type (WT) ID DISSOLVED ORGANIC-MATTER; NORTHERN ADRIATIC SEA; NEURAL-NETWORKS; OCEAN COLOR; LIGHT-SCATTERING; COASTAL WATERS; CASE-1 WATERS; CHLOROPHYLL-A; MERIS DATA; PHYTOPLANKTON AB Water-type (WT) definition as a function of biooptical properties has relevance to the exploitation of satellite ocean color data because it may provide a mean to optimize the atmospheric correction process or select the most appropriate bio-optical algorithm for the determination of optically significant constituents in seawater. Within such a framework, this paper defines a WT index assuming the existence of two extreme conditions. On one side, there are waters with optical properties totally depending on the phytoplankton component. On the other side, waters characterized by fully unrelated bio-optical quantities. The index of intermediate WTs is then defined on a statistical basis, and the resulting scheme is applied to a set of experimental data collected in an optically complex coastal region. Finally, in view of supporting remote sensing applications, a neural network algorithm is implemented to identify WTs using the normalized water leaving radiance. C1 Univ Maryland, Joint Ctr Earth Syst, NASA, GSFC, College Pk, MD 20742 USA. European Commiss, Global Environm Monitoring Unit, I-21020 Ispra, Italy. RP D'Alimonte, D (reprint author), Univ Maryland, Joint Ctr Earth Syst, NASA, GSFC, College Pk, MD 20742 USA. EM davide@ardbeg.gsfc.nasa.gov; giuseppe.zibordi@jrc.it; jean-francois.berthon@jrc.it OI D'Alimonte, Davide/0000-0001-7217-7057 NR 35 TC 23 Z9 23 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2007 VL 45 IS 8 BP 2644 EP 2651 DI 10.1109/TGRS.2007.896561 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 195NO UT WOS:000248419100025 ER PT J AU Warren, KM Weller, RA Sierawski, BD Reed, RA Mendenhall, MH Schrimpf, RD Massengill, LW Porter, ME Wilkinson, JD Label, KA Adams, JH AF Warren, Kevin M. Weller, Robert A. Sierawski, Brian D. Reed, Robert A. Mendenhall, Marcus H. Schrimpf, Ronald D. Massengill, Lloyd W. Porter, Mark E. Wilkinson, Jeffrey D. Label, Kenneth A. Adams, James H. TI Application of RADSAFE to model the single event upset response of a 0.25 mu m CMOS SRAM SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 9th European Workshop on Radiation and its Effects on Components and Systems CY SEP 27-29, 2006 CL Athens, GREECE DE GEANT4; heavy-ion; RADSAFE; SEU; TCAD ID CROSS-SECTION; INDUCED TRANSIENTS; CHARGE COLLECTION; NUCLEAR-REACTIONS; OPTOCOUPLERS; CIRCUITS; ENERGY; RATES AB The RADSAFE simulation framework is described and applied to model SEU in a 0.25 mu m CMOS 4 Mbit SRAM. For this circuit, the RADSAFE approach produces trends similar to those expected from classical rectangular parallelepiped models, but more closely represents the physical mechanisms responsible for SEU in the SRAM circuit. C1 Inst Space & Defense Elect, Nashville, TN 37203 USA. Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37203 USA. Vanderbilt Univ, Free Elect Laser Ctr, Nashville, TN 37203 USA. Medtron Microelect Ctr Inc, Tempe, AZ USA. Medtron CRDM Device Technol, Minneapolis, MN USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. RP Warren, KM (reprint author), Inst Space & Defense Elect, Nashville, TN 37203 USA. EM kevin.m.warren@vanderbilt.edu RI Wilkinson, Jeff/D-6309-2011; Schrimpf, Ronald/L-5549-2013; OI Schrimpf, Ronald/0000-0001-7419-2701; , Jeff/0000-0001-6454-0477 NR 22 TC 41 Z9 41 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2007 VL 54 IS 4 BP 898 EP 903 DI 10.1109/TNS.2006.889810 PN 2 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 203MC UT WOS:000248977700005 ER PT J AU Pease, RL Dunham, GW Seiler, JE Platteter, DG McClure, SS AF Pease, Ronald L. Dunham, Gary W. Seiler, John E. Platteter, Dale G. McClure, Steven S. TI Total dose and dose rate response of an AD590 temperature transducer SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 9th European Workshop on Radiation and its Effects on Components and Systems CY SEP 27-29, 2006 CL Athens, GREECE DE dose rate; enhanced low-dose-rate sensitivity; radiation effects; temperature transducer; total ionizing dose ID RATE SENSITIVITY; DEVICES AB The total dose response of the Analog Devices AD590 is presented for a variety of irradiation test conditions. The parts packaged in flat-packs show very large enhanced low dose rate sensitive (ELDRS) response for unbiased irradiation, starting at about 20 krad, whereas parts packaged in TO-52 cans are not ELDRS. The reason for this package sensitivity appears to be a result of hydrogen trapped in the cavity of the flat-pack package. The responses at 10 mrad/s and 3 mrad/s are essentially the same, indicating that the low dose rate enhancement factor has leveled off below 10 mrad/s. Elevated temperature irradiation at 100 degrees C and 5 rad/s does not simulate the low dose rate response. C1 RLP Res, Los Lunas, NM 87031 USA. NAVSEA Crane, Crane, IN 47522 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pease, RL (reprint author), RLP Res, Los Lunas, NM 87031 USA. EM rpease@rlpresearch.com; gdunham@atd.crane.navy.mil; seiler.john@atd.crane.navy.mil; platteter@atd.crane.navy.mil; steven.s.mcclure@jpl.nasa.gov NR 8 TC 16 Z9 16 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2007 VL 54 IS 4 BP 1049 EP 1054 DI 10.1109/TNS.2007.892262 PN 2 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 203MC UT WOS:000248977700028 ER PT J AU Mavromichalaki, H Papaioannou, A Mariatos, G Papailiou, M Belov, A Eroshenko, E Yanke, V Stassinopoulos, EG AF Mavromichalaki, H. Papaioannou, A. Mariatos, G. Papailiou, M. Belov, A. Eroshenko, E. Yanke, V. Stassinopoulos, E. G. TI Cosmic ray radiation effects on space environment associated to intense solar and geomagnetic activity SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 9th European Workshop on Radiation and its Effects on Components and Systems CY SEP 27-29, 2006 CL Athens, GREECE DE cosmic rays; extraterrestrial phenomena; solar radiation; Space weather ID FORBUSH DECREASES AB Intense cosmic ray fluxes during Forbush decreases can be responsible for a number of radiation effects in electronics and sensor systems of spacecrafts and aircrafts. Monitoring, modeling and possible prediction, from the real-time database of the Athens Neutron Monitor Data Processing (ANMODAP) Center are being considered. A different kind of cosmic ray events that evolves during a Forbush decrease, as an additional intermediate enhancement and its impact on electronic systems, is also identified. C1 Univ Athens, Dept Phys, Nucl & Particle Phys Sect, Athens, Greece. IZMIRAN, Inst Terr Magnetism Ionosphere & Radio Wave Propa, Troitsk 142092, Russia. NASA, Goddard Space Flight Ctr, Appl Engn & Technol Directorate, Radiat Phys Off, Greenbelt, MD 20771 USA. RP Mavromichalaki, H (reprint author), Univ Athens, Dept Phys, Nucl & Particle Phys Sect, Athens, Greece. EM emavromi@phys.uoa.gr; at-papaio@phys.uoa.gr; gmphysics@yahoo.com; mpapahl@phys.uoa.gr; abelov@izmiran.rssi.ru; erosh@izmiran.ru; yanke@izmiran.rssi.ru; estassin@pop100.gsf.nasa.gov RI Papaioannou, Athanasios/K-7065-2013 NR 26 TC 8 Z9 8 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2007 VL 54 IS 4 BP 1089 EP 1096 DI 10.1109/TNS.2007.897401 PN 2 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 203MC UT WOS:000248977700035 ER PT J AU Marshall, CJ Marshall, PW Howe, CL Reed, RA Weller, RA Mendenhall, A Waczynski, A Ladbury, R Jordan, TA AF Marshall, C. J. Marshall, P. W. Howe, C. L. Reed, R. A. Weller, R. A. Mendenhall, A. Waczynski, A. Ladbury, R. Jordan, T. A. TI Comparison of measured dark current distributions with calculated damage energy distributions in HgCdTe SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 9th European Workshop on Radiation and its Effects on Components and Systems CY SEP 27-29, 2006 CL Athens, GREECE DE CCD; dark current distribution; GEANT4; HgCdTe; proton effects ID SCREENED COULOMB SCATTERING; INDUCED DISPLACEMENT DAMAGE; IRRADIATED SILICON DEVICES; MICROVOLUMES; EXTREMES; GEANT4; CCDS AB This paper presents a combined Monte Carlo and analytic approach to the calculation of the pixel-to-pixel distribution of proton-induced damage in a HgCdTe sensor array and compares the results to measured dark current distributions after damage by 63 MeV protons. The moments of the Coulombic, nuclear elastic and nuclear inelastic damage distributions were extracted from Monte Carlo simulations and combined to form a damage distribution using the analytic techniques first described by Marshall et al The calculations show that the high energy recoils from the nuclear inelastic reactions (calculated using the Monte Carlo code MCNPX) produce a pronounced skewing of the damage energy distribution. While the nuclear elastic component (also calculated using the MCNPX) contributes only a small fraction of the total nonionizing damage energy, its inclusion in the shape of the damage across the array is significant. The Coulombic contribution was calculated using the Monte Carlo radiative energy desposition (MRED), a Geant4 application. The comparison with the dark current distribution strongly suggests that mechanisms which are not linearly correlated with nonionizing damage produced according to collision kinematics are responsible for the observed dark current increases. This has important implications for the process of predicting the on-orbit dark current response of the HgCdTe sensor array. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Vanderbilt Univ, Nashville, TN 37235 USA. Global Sci & Technol, Greenbelt, MD 20771 USA. EMPC, Gaithersburg, MD 20885 USA. RP Marshall, CJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM cmarsha112@aol.com NR 21 TC 5 Z9 5 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2007 VL 54 IS 4 BP 1097 EP 1103 DI 10.1109/TNS.2007.895804 PN 2 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 203MC UT WOS:000248977700036 ER PT J AU Johnston, AH Miyahira, TF AF Johnston, Allan H. Miyahira, Tetsuo F. TI Radiation damage in power MOSFET optocouplers SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 9th European Workshop on Radiation and its Effects on Components and Systems CY SEP 27-29, 2006 CL Athens, GREECE DE MOSFET; optocoupler; proton damage; space radiation effects ID ENERGY-DEPENDENCE; PROTON DAMAGE; DEGRADATION; TRANSIENTS AB Radiation damage is investigated in optocouplers with power MOSFET output stages. They differ from conventional optocouplers, incorporating an intermediate photovoltaic chip to allow the MOSFET gate voltage to be controlled by the light-emitting diode. These optocouplers are sensitive to ionization as well as displacement damage, and can fail catastrophically from degradation in either the power MOSFET or the LED. Radiation testing must take both mechanisms into account. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnston, AH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM allan.h.johnston@jpl.nasa.gov; tetsuo.f.miyahira@jpl.nasa.gov NR 13 TC 0 Z9 1 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2007 VL 54 IS 4 BP 1104 EP 1109 DI 10.1109/TNS.2007.903172 PN 2 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 203MC UT WOS:000248977700037 ER PT J AU Becker, HN Farr, WH Zhu, DQ AF Becker, Heidi N. Farr, William H. Zhu, David Q. TI Radiation response of emerging high gain, low noise detectors SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 9th European Workshop on Radiation and its Effects on Components and Systems CY SEP 27-29, 2006 CL Athens, GREECE DE avalanche photodiode; excess noise factor; internal discrete avalanche photodiode; photon counting ID AVALANCHE PHOTODIODES AB Data illustrating the radiation response of emerging high gain, low noise detectors are presented. Ionizing dose testing of silicon internal discrete avalanche photodiodes, and 51-MeV proton testing of InGaAs/InAIAs avalanche photodiodes operated in Geiger mode are discussed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Becker, HN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Heidi.N.Becker@jpl.nasa.gov; William.H.Farr@jpl.nasa.gov; David.Q.Zhu@jpl.nasa.gov NR 8 TC 5 Z9 5 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2007 VL 54 IS 4 BP 1129 EP 1135 DI 10.1109/TNS.2007.894179 PN 2 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 203MC UT WOS:000248977700041 ER PT J AU Peratt, AL Eastman, TE AF Peratt, Anthony L. Eastman, Timothy E. TI Special issue on space and cosmic plasma SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Editorial Material C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Perot Syst Corp, Greenbelt, MD 20771 USA. RP Peratt, AL (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. NR 9 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0093-3813 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD AUG PY 2007 VL 35 IS 4 BP 741 EP 744 DI 10.1109/TPS.2007.905079 PN 1 PG 4 WC Physics, Fluids & Plasmas SC Physics GA 199MT UT WOS:000248700600001 ER PT J AU Marquette, ML Byerly, D Sognier, M AF Marquette, Michele L. Byerly, Diane Sognier, Marguerite TI A novel in vitro three-dimensional skeletal muscle model SO IN VITRO CELLULAR & DEVELOPMENTAL BIOLOGY-ANIMAL LA English DT Article DE C2C12 cells; muscle; differentiation; three-dimensional; rotary cell culture system ID ROTATING-WALL VESSEL; EXTRACELLULAR-MATRIX; CELL-LINE; SIMULATED MICROGRAVITY; SATELLITE CELLS; DIFFERENTIATION; TISSUE; CULTURE; PROLIFERATION; CONSTRUCTS AB A novel three-dimensional (3D) skeletal muscle model composed of C2C12 mouse myoblasts is described. This model was generated by cultivating myoblasts in suspension using the rotary cell culture system (RCCS), a unique culture environment. Single-cell suspensions of myoblasts were seeded at 5x10(5)/ml in growth medium without exogenous support structures or substrates. Cell aggregation occurred in both RCCS and suspension control (SC) conditions within 12 h but occurred more rapidly in the SC at all time intervals examined. RCCS-cultured myoblasts fused and differentiated into a 3D construct without serum deprivation or alterations. Syncitia were quantified at 3 and 6+ d in stained thin sections. A significantly greater number of syncitia was found at 6+ d in the RCCS cultures compared to the SC. The majority of syncitia were localized to the periphery of the cell constructs for all treatments. The expression of sarcomeric myosin heavy chain (MHC) was localized at or near the periphery of the 3D construct. The majority of MHC was associated with the large cells (syncitia) of the 6+-d aggregates. These results show, for the first time, that myoblasts form syncitia and express MHC in the presence of growth factors and without the use of exogenous supports or substrates. This model test system is useful for investigating initial cell binding, myoblast fusion and syncitia formation, and differentiation processes. C1 Univ Texas, Med Branch, Dept Neurosci & Cell Biol, Galveston, TX 77550 USA. NASA, Lyndon B Johnson Space Ctr, Div Human Adaptat & Countermeasures, Houston, TX 77058 USA. Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. RP Marquette, ML (reprint author), Univ Texas, Med Branch, Dept Neurosci & Cell Biol, Galveston, TX 77550 USA. EM michele.marquette-1@nasa.gov2 NR 73 TC 10 Z9 10 U1 0 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 1071-2690 J9 IN VITRO CELL DEV-AN JI In Vitro Cell. Dev. Biol.-Anim. PD AUG PY 2007 VL 43 IS 7 BP 255 EP 263 DI 10.1007/s11626-007-9054-0 PG 9 WC Cell Biology; Developmental Biology SC Cell Biology; Developmental Biology GA 215BL UT WOS:000249782400007 PM 17786532 ER PT J AU Balint, TS Sturm, EJ Woolley, RC Jordan, JF AF Balint, Tibor S. Sturm, Erick J., II Woolley, Ryan C. Jordan, James F. TI Can we power future mars missions? SO JBIS-JOURNAL OF THE BRITISH INTERPLANETARY SOCIETY LA English DT Article DE Mars; Radioisotope Power Systems; RPS; RTG; ARPS; solar power; batteries; fission power; NASA AB The Vision for Space Exploration identified the exploration of Mars as one of the key pathways. In response, NASA's Mars Program Office is developing a detailed mission lineup for the next decade that would lead to future explorations. Mission architectures for the next decade include both orbiters and landers. Existing power technologies, which could include solar panels, batteries, radioisotope power systems, and in the future fission power, could support these missions. Second and third decade explorations could target human precursor and human in-situ missions, building on increasingly complex architectures. Some of these could use potential feed forward from earlier Constellation missions to the Moon, discussed in the ESAS study. From a potential Mars Sample Return mission to human missions the complexity of the architectures increases, and with it the delivered mass and power requirements also amplify. The delivered mass at Mars mostly depends on the launch vehicle, while the landed mass might be further limited by EDL technologies, including the aeroshell, parachutes, landing platform, and pinpoint landing. The resulting in-situ mass could be further divided into payload elements and suitable supporting power systems. These power systems can range from tens of watts to multi-kilowatts, influenced by mission type, mission configuration, landing location, mission duration, and season. Regardless, the power system design should match the power needs of these surface assets within a given architecture. Consequently, in this paper we will identify potential needs and bounds of delivered mass and architecture dependant power requirements to surface assets that would enable future in-situ exploration of Mars. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Balint, TS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 301-170U, Pasadena, CA 91109 USA. EM tibor.balint@jpl.nasa.gov NR 20 TC 0 Z9 0 U1 2 U2 7 PU BRITISH INTERPLANETARY SOC PI LONDON PA 27-29 S LAMBETH RD, LONDON SW8 1SZ, ENGLAND SN 0007-084X J9 JBIS-J BRIT INTERPLA JI JBIS-J. Br. Interplanet. Soc. PD AUG PY 2007 VL 60 IS 8 BP 294 EP 303 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Engineering; Astronomy & Astrophysics; Geology GA 188FZ UT WOS:000247906200004 ER PT J AU Whiteman, DN Veselovskii, I Cadirola, M Rush, K Comer, J Potter, JR Tola, R AF Whiteman, David N. Veselovskii, Igor Cadirola, Martin Rush, Kurt Comer, Joseph Potter, John R. Tola, Rebecca TI Demonstration measurements of water vapor, cirrus clouds, and carbon dioxide using a high-performance Raman lidar SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID INTERNATIONAL H2O PROJECT; ELASTIC-BACKSCATTER LIDAR; ATMOSPHERIC AEROSOL; PART I; EXTINCTION; IHOP-2002; PROFILES; TEMPERATURE; MOISTURE; SPECTRA AB Profile measurements of atmospheric water vapor, cirrus clouds, and carbon dioxide using the Raman Airborne Spectroscopic lidar ( RASL) during ground-based, upward-looking tests are presented here. These measurements improve upon any previously demonstrated using Raman lidar. Daytime boundary layer profiling of water vapor mixing ratio up to an altitude of approximately 4 km under moist, midsummer conditions is performed with less than 5% random error using temporal and spatial resolution of 2 min and 60-210 m, respectively. Daytime cirrus cloud optical depth and extinction-to-backscatter ratio measurements are made using a 1-min average. The potential to simultaneously profile carbon dioxide and water vapor mixing ratio through the boundary layer and extending into the free troposphere during the nighttime is also demonstrated. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. Ecotronics, Clarksburg, MD USA. Sci Syst & Applicat, Lanham, MD USA. Barr Associates, Westford, MA USA. RP Whiteman, DN (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1,Bldg 33,Room D404, Greenbelt, MD 20771 USA. EM david.n.whiteman@nasa.gov NR 34 TC 18 Z9 20 U1 1 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD AUG PY 2007 VL 24 IS 8 BP 1377 EP 1388 DI 10.1175/JTECH2058.1 PG 12 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 205FR UT WOS:000249099900005 ER PT J AU Heymsfield, AJ Schmitt, C Bansemer, A van Zadelhoff, GJ McGill, MJ Twohy, C Baumgardner, D AF Heymsfield, Andrew J. Schmitt, Carl Bansemer, Aaron van Zadelhoff, Gerd-Jan McGill, Matthew J. Twohy, Cynthia Baumgardner, Darrel TI Comments on "Effective radius of ice cloud particle populations derived from aircraft probes" - Reply SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Editorial Material ID CRYSTALS; CIRRUS; FSSP C1 Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Koninklijk Nederlands Meteorol Inst, De Bilt, Netherlands. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. Univ Nacl Autonoma Mexico, Ctr Ciencias Atmosfera, Mexico City 04510, DF, Mexico. RP Heymsfield, AJ (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM heyms1@ncar.ucar.edu RI Heymsfield, Andrew/E-7340-2011; McGill, Matthew/D-8176-2012; van Zadelhoff, Gerd-Jan/K-6283-2013; Schmitt, Carl/P-5490-2015 NR 19 TC 0 Z9 0 U1 0 U2 3 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 AUG PY 2007 VL 24 IS 8 BP 1511 EP 1518 DI 10.1175/JTECH2077.1 PG 8 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 205FR UT WOS:000249099900016 ER PT J AU Kim, SB Lee, T Fukumori, I AF Kim, Seung-Bum Lee, Tong Fukumori, Ichiro TI Mechanisms controlling the interannual variation of mixed layer temperature averaged over the Nino-3 region SO JOURNAL OF CLIMATE LA English DT Article ID EQUATORIAL PACIFIC-OCEAN; TROPICAL INSTABILITY WAVES; SEA-SURFACE TEMPERATURE; 1997-98 EL-NINO; CIRCULATION MODEL; CONCEPTUAL-MODEL; ATLANTIC-OCEAN; HEAT-BUDGET; PART I; VARIABILITY AB Processes controlling the interannual variation of mixed layer temperature (MLT) averaged over the Nino-3 domain (5 degrees N-5 degrees S, 150 degrees-90 degrees W) are studied using an ocean data assimilation product that covers the period of 1993-2003. The overall balance is such that surface heat flux opposes the MLT change but horizontal advection and subsurface processes assist the change. Advective tendencies are estimated here as the temperature fluxes through the domain's boundaries, with the boundary temperature referenced to the domain-averaged temperature to remove the dependence on temperature scale. This allows the authors to characterize external advective processes that warm or cool the water within the domain as a whole. The zonal advective tendency is caused primarily by large-scale advection of warm-pool water through the western boundary of the domain. The meridional advective tendency is contributed to mostly by Ekman current advecting large-scale temperature anomalies through the southern boundary of the domain. Unlike many previous studies, the subsurface processes that consist of vertical mixing and entrainment are explicitly evaluated. In particular, a rigorous method to estimate entrainment allows an exact budget closure. The vertical mixing across the mixed layer (ML) base has a contribution in phase with the MLT change. The entrainment tendency due to the temporal change in ML depth is negligible compared to other subsurface processes. The entrainment tendency by vertical advection across the ML base is dominated by large-scale changes in upwelling and the temperature of upwelling water. Tropical instability waves (TIWs) result in smaller-scale vertical advection that warms the domain during La Nina cooling events. However, such a warming tendency is overwhelmed by the cooling tendency associated with the large-scale upwelling by a factor of 2. In summary, all the balance terms are important in the MLT budget except the entrainment due to lateral induction and temporal variation in ML depth. All three advective tendencies are primarily caused by large-scale and low-frequency processes, and they assist the Nino-3 MLT change. When the advective tendencies are evaluated by spatially averaging the conventional local advection of temperature, the apparent effects of currents with spatial scales smaller than the domain (such as TIWs) become very important as they redistribute heat within the Nino-3 domain. As a result, for example, the averaged zonal advective tendency counteracts rather than assists the Nino-3 MLT change. However, such internal redistribution of heat does not represent external processes that control the domain-averaged MLT. C1 CALTECH, Jet Propuls Lab, Pasadena, CA USA. RP Kim, SB (reprint author), Remote Sensing Syst, 438 First St,Suite 200, Santa Rosa, CA 95401 USA. EM kim@remss.com NR 39 TC 48 Z9 48 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD AUG 1 PY 2007 VL 20 IS 15 BP 3822 EP 3843 DI 10.1175/JCLI4206.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 198IH UT WOS:000248619800007 ER PT J AU Kumar, A Jha, B Zhang, Q Bounoua, L AF Kumar, Arun Jha, Bhaskar Zhang, Qin Bounoua, Lahouari TI A new methodology for estimating the unpredictable component of seasonal atmospheric variability SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODEL; SOIL-MOISTURE; GCM SIMULATIONS; POTENTIAL PREDICTABILITY; SURFACE TEMPERATURES; NATURAL VARIABILITY; NORTH-AMERICA; ENSEMBLE; PREDICTION; CLIMATE AB Predictability limits for seasonal atmospheric climate variability depend on the fraction of variability that is due to factors external to the atmosphere (e.g., boundary conditions) and the fraction that is internal. From the analysis of observed data alone, however, separation of the total seasonal atmospheric variance into its external and internal components remains a difficult and controversial issue. In this paper a simple procedure for estimating atmospheric internal variability is outlined. This procedure is based on the expected value of the mean square error between the observed and the general circulation model simulated (or predicted) seasonal mean anomaly. The end result is a spatial map for the estimate of the observed seasonal atmospheric internal (or unpredictable) variability. As improved general circulation models become available, mean square error estimated from the new generation of general circulation models can be easily included in the procedure proposed herein, bringing the estimate for the internal variability closer to its true estimate. C1 NCEP NOAA, Climate Predict Ctr, Camp Springs, MD USA. NCEP NOAA, RSIS, Climate Predict Ctr, Camp Springs, MD USA. Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD USA. RP Kumar, A (reprint author), Climate Predict Ctr, 5200 Auth Rd,Rm 800, Camp Springs, MD 20746 USA. EM arun.kumar@noaa.gov NR 36 TC 27 Z9 27 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD AUG 1 PY 2007 VL 20 IS 15 BP 3888 EP 3901 DI 10.1175/JCLI4216.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 198IH UT WOS:000248619800010 ER PT J AU Zaitchik, BF Evans, JP Geerken, RA Smith, RB AF Zaitchik, Benjamin F. Evans, Jason P. Geerken, Roland A. Smith, Ronald B. TI Climate and vegetation in the Middle East: Interannual variability and drought feedbacks SO JOURNAL OF CLIMATE LA English DT Article ID SEMI-ARID REGIONS; LAND-ATMOSPHERE INTERACTIONS; SOIL-MOISTURE; RANGELAND VEGETATION; JULY CIRCULATION; SURFACE ALBEDO; BOUNDARY-LAYER; PRECIPITATION FEEDBACK; MESOSCALE MODEL; NDVI AB The Euphrates Plain (EP) experiences large interannual variability in vegetation cover, especially in areas of marginal rain-fed agriculture. Vegetation in this region is primarily limited by available soil moisture, as determined by winter precipitation, spring precipitation, and air temperature. Satellite analyses indicate that the springtime normalized difference vegetation index (NDVI) is negatively correlated with surface albedo, and that interannual variability in albedo in the EP produces an estimated forcing on the radiation balance that peaks at 16.0 W m(-2) in May. Simulations with a regional climate model indicate that surface energy fluxes during a drought year (1999) differed substantially from those during a year with normal precipitation (2003). These differences were geographically specific, with the EP exhibiting increased albedo and decreased sensible heat flux while the neighboring Zagros Plateau region showed no albedo effect, a large increase in sensible heat flux, and an offsetting reduction in latent heat flux. In both the EP and the Zagros there was a potential for positive feedbacks on temperature and drought in late spring, though the most likely feedback mechanisms differed between the two regions: in the EP surface brightening leads to cooling and reduced turbulent heat flux, while in the Zagros region reduced latent heat flux leads to warming and a deepening of the planetary boundary layer. C1 Yale Univ, Dept Geol & Geophys, New Haven, CT USA. RP Zaitchik, BF (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 614-3, Greenbelt, MD 20771 USA. EM bzaitchik@hsb.gsfc.nasa.gov RI Evans, Jason/F-3716-2011; Zaitchik, Benjamin/B-9461-2013 OI Evans, Jason/0000-0003-1776-3429; NR 69 TC 24 Z9 24 U1 2 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD AUG 1 PY 2007 VL 20 IS 15 BP 3924 EP 3941 DI 10.1175/JCLI4223.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 198IH UT WOS:000248619800012 ER PT J AU Gu, GJ Adler, RF Huffman, GJ Curtis, S AF Gu, Guojun Adler, Robert F. Huffman, George J. Curtis, Scott TI Tropical rainfall variability on interannual-to-interdecadal and longer time scales derived from the GPCP monthly product SO JOURNAL OF CLIMATE LA English DT Article ID SEA-SURFACE TEMPERATURE; EL-NINO; SOUTHERN-OSCILLATION; PRECIPITATION; PACIFIC; CLIMATE; TRENDS; ENSO; PINATUBO; ERUPTION AB Global and large regional rainfall variations and possible long-term changes are examined using the 27-yr (1979-2005) Global Precipitation Climatology Project (GPCP) monthly dataset. Emphasis is placed on discriminating among variations due to ENSO, volcanic events, and possible long-term climate changes in the Tropics. Although the global linear change of precipitation in the dataset is near zero during the time period, an increase in tropical rainfall is noted in the dataset, with a weaker decrease over Northern Hemisphere middle latitudes. Focusing on the Tropics (25 degrees S-25 degrees N), the dataset indicates ail upward linear change (0.06 mm day(-1) decade(-1)) and a downward linear change (-0.01 ram day(-1) decade(-1)) over tropical ocean and land, respectively. This corresponds to an about 5.5% increase (ocean) and 1% decrease (land) during the entire 27-yr time period. The year 2005 has the largest annual tropical total precipitation (land plus ocean) for the GPCP record. The five highest years are (in descending order) 2005, 2004, 1998, 2003, and 2002. For tropical ocean the five highest years are 1998, 2004, 2005, 2002, and 2003. Techniques are applied to isolate and quantity variations due to ENSO and two major volcanic eruptions during the time period (El Chichon, March 1982; Mount Pinatubo, June 1991) in order to examine longer-time-scale changes. The ENSO events generally do not impact the tropical total rainfall, but rather induce significant anomalies with opposite signs over tropical land and ocean. The impact of the two volcanic eruptions is estimated to be about a 5% reduction in tropical rainfall over both land and ocean. A modified dataset (with ENSO and volcano effects removed) retains the same approximate linear change slopes, but with reduced variances, thereby increasing the statistical significance levels associated with the long-term rainfall changes in the Tropics. However, although care has been taken to ensure that this dataset is as homogeneous as possible, firm establishment of the existence of the discussed changes as long-term trends may require continued analysis of the input datasets and a lengthening of the observation period. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD USA. RP Gu, GJ (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA. EM ggu@agnes.gsfc.nasa.gov RI Curtis, Scott/C-1115-2013; Huffman, George/F-4494-2014; OI Huffman, George/0000-0003-3858-8308; Curtis, Scott/0000-0001-9065-8639 NR 37 TC 102 Z9 104 U1 0 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD AUG 1 PY 2007 VL 20 IS 15 BP 4033 EP 4046 DI 10.1175/JCLI4227.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 198IH UT WOS:000248619800019 ER PT J AU Malte, H Larsen, C Musyl, M Brill, R AF Malte, Hans Larsen, Christina Musyl, Michael Brill, Richard TI Differential heating and cooling rates in bigeye tuna (Thunnus obesus Lowe): a model of non-steady state heat exchange SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE archival tag; endothermy; Scombridae; swimming speed; temperature; thermoregulation; vertical movement ID SKIPJACK KATSUWONUS-PELAMIS; ARCHIVAL TAGGING DATA; LARGE WATER TUNNEL; BLUEFIN TUNA; YELLOWFIN TUNA; SWIMMING PERFORMANCE; PHYSIOLOGICAL THERMOREGULATION; HORIZONTAL MOVEMENTS; ULTRASONIC TELEMETRY; MUSCLE TEMPERATURE AB We analyzed water temperature, visceral cavity temperature and depth data from archival tags retrieved from bigeye tuna (Thunnus obesus) at liberty in the central Pacific for up to 57 days using a mathematical model of heat exchange. Our model took into account the transfer of heat between the portions of the myotomes comprising red muscle fibers adjacent to the spinal column and served by vascular counter current heat exchanges (henceforth referred to as 'red muscle') and the water, as well as between the red muscle and the temperature sensor of the archival tags in the visceral cavity. Our model successfully predicted the recorded visceral cavity temperatures during vertical excursions provided that the rate constants for heat transfer between the ambient water and the red muscle during cooling (k(low)) and those during heating (k(high)) were very dissimilar. Least-squares fitting of klow and khigh for the entire period that the fish were at liberty yielded values generally in the ranges 0.02 - 0.04 min(-1) and 0.2 - 0.6 min(-1) (respectively), with an average ratio k(high)/k(low) of approximate to 12. Our results confirmed those from previous studies showing that bigeye tuna have extensive physiological thermoregulatory abilities probably exerted through changes of blood flow patterns that controlled the efficiency of vascular countercurrent heat exchanges. There was a small but significant negative correlation between klow and size, whereas there was no correlation between khigh and size. The maximum swimming speeds during vertical excursions (calculated from the pressure data) occurred midway during ascents and averaged approximate to 2 FL s(-1) (where FL=fork length), although speeds as high approximate to 4 - 7 FL s(-1) were also noted. C1 Univ Aarhus, Inst Biol Sci, Dept Zoophysiol, DK-8000 Aarhus C, Denmark. Univ Hawaii, Joint Inst Marine & Atmospher Res, Pelag Fisheries Res Program, Honolulu, HI 96822 USA. NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Honolulu Lab, Honolulu, HI 96822 USA. RP Brill, R (reprint author), Univ Aarhus, Inst Biol Sci, Dept Zoophysiol, DK-8000 Aarhus C, Denmark. EM rbrill@vims.edu RI Malte, Hans/J-6018-2013 NR 53 TC 15 Z9 15 U1 1 U2 17 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD AUG 1 PY 2007 VL 210 IS 15 BP 2618 EP 2626 DI 10.1242/jeb.003855 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 205LT UT WOS:000249116000013 PM 17644676 ER PT J AU Tunstel, E AF Tunstel, Edward TI Operational performance metrics for mars exploration Rovers SO JOURNAL OF FIELD ROBOTICS LA English DT Article; Proceedings Paper CT 4th IEEE International Workshop on Safety Security and Rescue Robots/6th Performance Metrics for Intelligent Systems CY AUG, 2006 CL Nat Inst Stand Tech, Gaithersburg, MD SP IEEE HO Nat Inst Stand Tech AB The concept of operational performance metrics and associated measurement issues is explored for deployed robotic systems. The focus is on performance of mobility and robotic arm autonomy exercised on the NASA Mars Exploration Rovers surface mission. This planetary rover mission has been underway for nearly 3 years since January 2004 using two rovers performing separate missions. The autonomy functions of surface navigation, short-distance approach to surface science targets, and robotic placement of arm-mounted instruments on science targets are considered. Operational metrics that measure performance of these functions relative to system requirements are advocated. Specific metrics are defined and computed using telemetry from the rovers' multiyear operations on Mars and applied to rate performance during their respective missions. An existing methodology is applied to compute metrics with respect to required performance and to aggregate multiple metrics into a composite performance score for each rover. The formulation is augmented to accommodate importance weights that add flexibility in use of the metrics by different potential endusers, e.g., sponsors, program managers, systems engineers, and technologists. A brief example illustrates the application and effect of importance weights on overall rover performance scores. (c) 2007 whey Periodicals, Inc. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tunstel, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM tunstel@robotics.jpl.nasa.gov NR 36 TC 5 Z9 5 U1 0 U2 3 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1556-4959 J9 J FIELD ROBOT JI J. Field Robot. PD AUG-SEP PY 2007 VL 24 IS 8-9 BP 651 EP 670 DI 10.1002/rob.20205 PG 20 WC Robotics SC Robotics GA 214PS UT WOS:000249751200003 ER PT J AU Balasubramanyam, MS Chen, CP Trinh, HP AF Balasubramanyam, M. S. Chen, C. P. Trinh, H. P. TI A new finite-conductivity droplet evaporation model including liquid turbulence effect SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME LA English DT Article DE evaporation; spray; numerical modeling ID VAPORIZATION MODEL; SPRAY CALCULATIONS; PRESSURE AB A new approach to account for finite thermal conductivity and turbulence effects within atomizing droplets of an evaporating spray is presented in this paper The model is an extension of the T-blob and T-TAB atomization/spray model of Trinh and Chen [Atomization and Sprays, 16(8), pp. 907-932]. This finite conductivity model is based on the two-temperature film theory in which the turbulence characteristics of the droplet are used to estimate the effective thermal diffusivity for the liquid-side film thickness. Both one-way and two-way coupled calculations were performed to investigate the performance of this model against the published experimental data. C1 Univ Alabama, Dept Chem & Mat Engn, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Engn Directorate, Huntsville, AL 35812 USA. RP Chen, CP (reprint author), Univ Alabama, Dept Chem & Mat Engn, Huntsville, AL 35899 USA. EM cchen@che.uah.edu NR 21 TC 7 Z9 7 U1 0 U2 3 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0022-1481 J9 J HEAT TRANS-T ASME JI J. Heat Transf.-Trans. ASME PD AUG PY 2007 VL 129 IS 8 BP 1082 EP 1086 DI 10.1115/1.2737481 PG 5 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 207PG UT WOS:000249262400027 ER PT J AU Curtis, S Salahuddin, A Adler, RF Huffman, GJ Gu, GJ Hong, Y AF Curtis, Scott Salahuddin, Ahmed Adler, Robert F. Huffman, George J. Gu, Guojun Hong, Yang TI Precipitation extremes estimated by GPCP and TRMM: ENSO relationships SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article; Proceedings Paper CT 5th International Science Conference on the Global Energy and Water Cycle CY JUN 24, 2005 CL Costa Mesa, CA ID ATLANTIC CONVERGENCE ZONE; CONTIGUOUS UNITED-STATES; EL-NINO; RAINFALL; VARIABILITY; EVENTS; CLIMATE; SATELLITE; PATTERNS; TEMPERATURE AB Global monthly and daily precipitation extremes are examined in relation to the El Nino-Southern Oscillation phenomenon. For each month around the annual cycle and in each 2.5 degrees grid block, extremes in the Global Precipitation Climatology Project dataset are defined as the top five (wet) and bottom five (dry) mean rain rates from 1979 to 2004. Over the tropical oceans El Nino-Southern Oscillation events result in a spatial redistribution and overall increase in extremes. Restricting the analysis to land shows that El Nino is associated with an increase in frequency of dry extremes and a decrease in wet extremes resulting in no change in net extreme months. During La Nina an increase in frequency of dry extremes and no change in wet extremes are observed. Thus, because of the juxtaposition of tropical land areas with the ascending branches of the global Walker Circulation, El Nino (La Nina) contributes to generally dry (wet) conditions in these land areas. In addition, daily rain rates computed from the Tropical Rainfall Measuring Mission Multisatellite Precipitation Analysis are used to define extreme precipitation frequency locally as the number of days within a given season that exceeded the 95th percentile of daily rainfall for all seasons (1998-2005). During this period, the significant relationships between extreme daily precipitation frequency and Nino-3.4 in the Tropics are spatially similar to the significant relationships between seasonal mean rainfall and Nino-3.4. However, to address the shortness of the record extreme daily precipitation frequency is also related to seasonal rainfall for the purpose of identifying regions where positive seasonal rainfall anomalies can be used as proxies for extreme events. Finally, the longer (1979-2005) but coarser Global Precipitation Climatology Project analysis is reexamined to pinpoint regions likely to experience an increase in extreme precipitation during El Nino-Southern Oscillation events. Given the significance of El Nino-Southern Oscillation predictions, this information will enable the efficient use of resources in preparing for and mitigating the adverse effects of extreme precipitation. C1 E Carolina Univ, Atmospher Sci Lab, Dept Geog, Greenville, NC 27858 USA. E Carolina Univ, Atmospher Sci Lab, Coastal Resources Management, Dept Geog, Greenville, NC 27858 USA. NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD USA. NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA. RP Curtis, S (reprint author), E Carolina Univ, Atmospher Sci Lab, Dept Geog, Brewster A232, Greenville, NC 27858 USA. EM curtisw@ecu.edu RI Hong, Yang/D-5132-2009; Curtis, Scott/C-1115-2013; Huffman, George/F-4494-2014; OI Hong, Yang/0000-0001-8720-242X; Huffman, George/0000-0003-3858-8308; Curtis, Scott/0000-0001-9065-8639 NR 37 TC 28 Z9 30 U1 2 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2007 VL 8 IS 4 BP 678 EP 689 DI 10.1175/JHM601.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 208YF UT WOS:000249354400004 ER PT J AU Schnase, JL Cushing, J Smith, JA AF Schnase, John L. Cushing, Judy Smith, James A. TI Biodiversity and ecosystem informatics SO JOURNAL OF INTELLIGENT INFORMATION SYSTEMS LA English DT Article DE biodiversity; ecosystems; informatics; ecological forecasting AB The field of Biodiversity and Ecosystem Informatics (BDEI) brings together computer scientists, biologists, natural resource managers, and others who wish to solve real-world challenges while advancing the underlying ecological, computer, and information sciences. The potential for synergies among these disciplines is high, because our need to understand complex, ecosystem-scale processes requires the solution to many groundbreaking technological problems. Fortunately, we are beginning to see increased support for applied computer science and information technology research in the context of environmental problem-solving. In July, 2001, the National Science Foundation (NSF), in collaboration with the United States Geological Survey (USGS), and the National Aeronautics and Space Administration (NASA), invited proposals for high-risk, small-scale planning and incubation activities to catalyze innovation and rapid advances in this new research community. The papers included in this special issue are selected, peer-reviewed summaries from principal investigators involved in this first NSF BDEI effort. These papers provide an overview of this emerging area and remind us that computer and information science and engineering play a crucial role in creating the technologies from which advances in the natural sciences evolve. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Evergreen State Coll, Olympia, WA 98505 USA. RP Schnase, JL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM John.L.Schnase@nasa.gov; JudyC@evergreen.edu; James.A.Smith@nasa.gov NR 3 TC 3 Z9 3 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0925-9902 J9 J INTELL INF SYST JI J. Intell. Inf. Syst. PD AUG PY 2007 VL 29 IS 1 BP 1 EP 6 DI 10.1007/s10844-006-0027-7 PG 6 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems SC Computer Science GA 201DF UT WOS:000248811000001 ER PT J AU Liu, YH Mavroidis, C Bar-Cohen, Y Chang, Z AF Liu, Yinghui Mavroidis, Constantinos Bar-Cohen, Yoseph Chang, Zensheu TI Analytical and experimental study of determining the optimal number of wedge shape cutting teeth in coring bits used in percussive drilling SO JOURNAL OF MANUFACTURING SCIENCE AND ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article; Proceedings Paper CT ASME Design Engineering Technical Conferences/Computers and Information in Engineering Conferences (DETC 2005) CY SEP 24-28, 2005 CL Long Beach, CA SP ASME ID ROCK; PENETRATION AB In this paper we study the design of the coring bits with wedge-shape cutting teeth of vibratory drills that percussively penetrate into brittle material. The overall coring bit specific energy is analytically derived as a function of the cutting teeth spacing and teeth number It is found that given the coring bit dimensions and rock material properties, there exist an optimal spacing/depth ratio and an optimal tooth number that minimize the coring bit specific energy and hence maximize the coring bit's drilling rate. Experimental drilling tests were performed to corroborate the analytical results. It was shown that the laboratory drilling tests follow the trend predicted by the theoretical analysis. C1 Northeastern Univ, Dept Mech & Ind Engn, Boston, MA 02115 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP Mavroidis, C (reprint author), Northeastern Univ, Dept Mech & Ind Engn, 360 Huntington Ave, Boston, MA 02115 USA. EM mavro@coe.neu.edu; yosi@jpl.nasa.gov NR 12 TC 3 Z9 3 U1 1 U2 3 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1087-1357 J9 J MANUF SCI E-T ASME JI J. Manuf. Sci. Eng.-Trans. ASME PD AUG PY 2007 VL 129 IS 4 BP 760 EP 769 DI 10.1115/1.2515345 PG 10 WC Engineering, Manufacturing; Engineering, Mechanical SC Engineering GA 206HP UT WOS:000249174800011 ER PT J AU Currie, JR Batra, AK Alim, MA Aggarwal, MD Lal, RB AF Currie, James R. Batra, Ashok K. Alim, Mohammad A. Aggarwal, Manmohan D. Lal, Ravindra B. TI Impedance studies of polycrystalline tin oxide (vol 18, pg 433, 2007) SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS LA English DT Correction C1 Alabama A&M Univ, Dept Elect Engn, Normal, AL 35762 USA. NASA, George C Marshall Space Flight Ctr, Avion Dept, Huntsville, AL 35812 USA. Alabama A&M Univ, Dept Phys, Normal, AL 35762 USA. RP Alim, MA (reprint author), Alabama A&M Univ, Dept Elect Engn, POB 297, Normal, AL 35762 USA. EM ashok.batra@email.aamu.edu; mohammad.alim@aamu.edu NR 1 TC 4 Z9 4 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0957-4522 J9 J MATER SCI-MATER EL JI J. Mater. Sci.-Mater. Electron. PD AUG PY 2007 VL 18 IS 8 BP 899 EP 899 DI 10.1007/s10854-007-9264-y PG 1 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA 180OV UT WOS:000247376200016 ER PT J AU Toda, R Yang, EH AF Toda, Risaku Yang, Eui-Hyeok TI A normally latched, large-stroke, inchworm microactuator SO JOURNAL OF MICROMECHANICS AND MICROENGINEERING LA English DT Article; Proceedings Paper CT 19th IEEE International Conference on Micro Electro Mechanical Systems (MEMS 2006) CY JAN 22-26, 2006 CL Istanbul, TURKEY SP IEEE, Robot & Automat Soc ID ACTUATOR; DESIGN; MOTOR AB This paper presents the successful demonstration of a large-stroke, high-precision inchworm microactuator. The actuator is capable of zero-power latching, or forcibly maintaining its position by using pre-stressed spring load. The actuator is driven by a combination of a PZT-stack actuator unit for slider thrust and electrostatic comb-drive units for slider grip. Incremental step size is precisely adjustable to the tens of nanometers level by controlling the PZT-stack actuator voltage. The observed minimum step size was 59 nm/cycle. Large stroke is obtained by repeating the operation sequence numerous times. A large-stroke actuation exceeding 600 mu m has been demonstrated. There is no conceivable limit to the stroke except for the length of the slider and external load. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Toda, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Risaku.Toda@jpl.nasa.gov OI Yang, Eui-Hyeok/0000-0003-4893-1691 NR 18 TC 10 Z9 10 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0960-1317 J9 J MICROMECH MICROENG JI J. Micromech. Microeng. PD AUG PY 2007 VL 17 IS 8 BP 1715 EP 1720 DI 10.1088/0960-1317/17/8/039 PG 6 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Instruments & Instrumentation; Physics, Applied SC Engineering; Science & Technology - Other Topics; Instruments & Instrumentation; Physics GA 200QB UT WOS:000248776800038 ER PT J AU Serizawa, H Fujita, D Lewinsohn, CA Singh, M Murakawa, H AF Serizawa, H. Fujita, D. Lewinsohn, C. A. Singh, M. Murakawa, H. TI Numerical analysis of mechanical testing for evaluating shear strength of SiC/SiC composite joints SO JOURNAL OF NUCLEAR MATERIALS LA English DT Article; Proceedings Paper CT 12th International Conference on Fusion Reactor Materials (ICFRM-12) CY DEC 07-12, 2005 CL Santa Barbara, CA ID INTERFACE AB As examples of the most typical methods to determine the shear strength of SiC/SiC composite joints, the asymmetrical four point bending test of a butt-joined composite, the tensile test of a lap-joined composite, and the compression test of a double-notched composite joint were analyzed by using a finite element method with the interface element. From the results, it was found that the shear strength in the asymmetrical bending test was controlled by both the surface energy and the shear strength at the interface regardless of their combination while the strength in the tensile test or the compression test was governed by the surface energy when both the surface energy and the shear strength were large. Also, the apparent shear strength of the composite joint obtained experimentally appeared to be affected by the combination of the surface energy and the shear strength at the interface. (c) 2007 Elsevier B-V. All rights reserved. C1 Osaka Univ, Joining & Welding Res Inst, Osaka 5670047, Japan. Ceramatec Inc, Salt Lake City, UT 84119 USA. NASA, Glenn Res Ctr, Ceram Branch, Cleveland, OH 44135 USA. RP Serizawa, H (reprint author), Osaka Univ, Joining & Welding Res Inst, 11-1 Mihogaoka, Osaka 5670047, Japan. EM serizawa@jwri.osaka-u.ac.jp NR 10 TC 7 Z9 7 U1 1 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-3115 J9 J NUCL MATER JI J. Nucl. Mater. PD AUG 1 PY 2007 VL 367 BP 1223 EP 1227 DI 10.1016/j.jnucmat.2007.03.223 PN B PG 5 WC Materials Science, Multidisciplinary; Nuclear Science & Technology SC Materials Science; Nuclear Science & Technology GA 204ZW UT WOS:000249083500061 ER PT J AU Chao, WC AF Chao, Winston C. TI Chimeric equatorial waves as a better descriptor for "convectively coupled equatorial waves" SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN LA English DT Article ID ROSSBY-GRAVITY-WAVES; TROPICAL INTRASEASONAL OSCILLATION; FREQUENCY DOMAIN; KELVIN WAVES; DISTURBANCES; MECHANISM; PACIFIC; ORIGIN; MODEL AB The term "convectively-coupled Kelvin waves" is misleading. That is because these waves have Rossby-wave components, comparable to their Kelvin-wave components and, in fact, bear a close resemblance to the Gill solution with a moving heating source. A better alternative would be to call these waves chimeric Kelvin waves, to signify their combined nature and the fact that they are implicitly convectively-coupled. By extension, chimeric Rossby waves and chimeric mixed Rossby-gravity waves would be better alternatives to "convectively-coupled Rossby waves" and "convectively-coupled mixed Rossby-gravity waves," respectively. Collectively, these waves can be called chimeric equatorial waves. Recognizing the above misleading terms can help avoid confusion. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Chao, WC (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Mail Code 613-2, Greenbelt, MD 20771 USA. EM Winston.c.chao@nasa.gov NR 17 TC 5 Z9 5 U1 0 U2 0 PU METEOROLOGICAL SOC JAPAN PI TOKYO PA C/O JAPAN METEOROLOGICAL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO, 100-0004, JAPAN SN 0026-1165 EI 2186-9057 J9 J METEOROL SOC JPN JI J. Meteorol. Soc. Jpn. PD AUG PY 2007 VL 85 IS 4 BP 521 EP 524 DI 10.2151/jmsj.85.521 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 221OQ UT WOS:000250237600006 ER PT J AU Juergensmeyer, MA Nelson, ES Juergensmeyer, EA AF Juergensmeyer, M. A. Nelson, E. S. Juergensmeyer, E. A. TI Shaking alone, without concurrent aeration, affects the growth characteristics of Escherichia coli SO LETTERS IN APPLIED MICROBIOLOGY LA English DT Article DE clinostat; E. coli; modeled microgravity; oxygenation of media; vibration ID BACILLUS-SUBTILIS; BACTERIAL-GROWTH; SPACE-FLIGHT; MICROGRAVITY AB Aims: This study investigated the effects of linear vibration on cultures grown in both hard- and soft-sided containers to determine whether vibration alone affected the growth rate. Methods and Results: Cultures of Escherichia coli were exposed to vibrational acceleration with and without access to additional oxygen. Vibrated cultures grown in hard-sided containers exited lag phase earlier and had a higher final yield than identical unshaken cultures, whether or not the cultures had access to ambient air. Cultures grown in soft-sided containers showed no response to vibration. Conclusions: Vibration in hard-sided containers decreases the length of the lag phase and increases final OD in E. coli, with or without increased oxygenation. Increased mixing and improved suspension, which result from vibration of cultures in hard-sided containers, are the most likely physical mechanisms for the more favorable culture conditions. Significance and Impact of the Study: This paper demonstrates that growth enhancement of shaken cultures is a function of the rigidity of the vessel even without aeration of the medium. C1 IIT, Res Inst, Chicago, IL 60616 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. Judson Coll, Elgin, IL USA. RP Juergensmeyer, MA (reprint author), IIT, Res Inst, 10 W 35th St, Chicago, IL 60616 USA. EM mjuergensmeyer@iitri.org NR 17 TC 5 Z9 5 U1 2 U2 2 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0266-8254 J9 LETT APPL MICROBIOL JI Lett. Appl. Microbiol. PD AUG PY 2007 VL 45 IS 2 BP 179 EP 183 DI 10.1111/j.1472-765X.2007.02172.x PG 5 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 209GM UT WOS:000249377000011 PM 17651215 ER PT J AU Bogard, DD Park, J AF Bogard, Donald D. Park, Jisun TI Excess Ar-40 in the Zagami shergottite: Does it reveal crystallization history? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID METEORITE; PYROXENES; MARS C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 7 TC 3 Z9 3 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A21 EP A21 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800024 ER PT J AU Dominguez, G Trigo-Rodriguez, JM Burchell, MJ Horz, F Llorca, J Tsou, P Anderson, B AF Dominguez, Gerardo Trigo-Rodriguez, Josep M. Burchell, Mark J. Horz, Fred Llorca, Jordi Tsou, Peter Anderson, Bill TI Analysis of factors contributing to bulbous capture tracks from cometary dust particles in Stardust aerogel collector SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID IMPACT C1 Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA. CSIC, Inst Space Sci, Barcelona 08193, Spain. IEEC, Barcelona 08034, Spain. Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Politecn Catalunya, Inst Tecn Energet, E-08028 Barcelona, Spain. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Los Alamos Natl Lab, Dynam & Energet Mat Div, Los Alamos, NM 87545 USA. EM gdominguez@ucsd.edu RI Llorca, Jordi/M-8134-2014 OI Llorca, Jordi/0000-0002-7447-9582 NR 5 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A37 EP A37 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800056 ER PT J AU Ganguly, J Ito, M Zhang, XY AF Ganguly, J. Ito, M. Zhang, X.-Y TI Mn-Cr decay system: Diffusion kinetics in pyroxenes and thermochronology of early solar system processes in meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM gunguly@email.arizona.edu RI Ganguly, Jibamitra/K-6795-2012 NR 4 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A53 EP A53 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800089 ER PT J AU Gibson, EK Mckay, DS Clemett, SJ Thomas-Keprta, KL Wentworth, SJ Robert, F Verchovsky, AB Wright, IP Pillinger, CT Rice, T Van Leer, B Meibom, A Mostefaoui, SM Socki, R Le, L AF Gibson, E. K. McKay, D. S. Clemett, S. J. Thomas-Keprta, K. L. Wentworth, S. J. Robert, F. Verchovsky, A. B. Wright, I. P. Pillinger, C. T. Rice, T. Van Leer, B. Meibom, A. Mostefaoui, S. M. Socki, R. Le, L. TI Identification and analysis of in situ carbon-bearing phases in Nakhla SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID AQUEOUS ALTERATION; MARS C1 NASA, KR, ARES, JSC, Houston, TX 77058 USA. Jacobs Engn, Houston, TX USA. CNRS, Museum Hist Nat, LEME, Paris, France. Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England. FEI Co, Hillsboro, OR 97124 USA. EM everett.k.gibson@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A55 EP A55 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800093 ER PT J AU Guo, W Perronnet, N Zolensky, ME Eiler, JM AF Guo, W. Perronnet, Ni. Zolensky, M. E. Eiler, J. M. TI Temperatures of aqueous alteration on carbonaceous chondrite parent bodies SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID OXYGEN; CARBONATES C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM wfguo@gps.caltech.edu RI Guo, Weifu/E-8876-2010 NR 12 TC 1 Z9 1 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A61 EP A61 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800104 ER PT J AU Heber, VS Baur, H Burnett, DS Reisenfeld, DB Wieler, R Wiens, RC AF Heber, V. S. Baur, H. Burnett, D. S. Reisenfeld, D. B. Wieler, R. Wiens, R. C. TI Light noble gas composition of different solar wind regimes: results from genesis SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 ETH, Isotope Geol & Mineral Resources, NW C, CH-8092 Zurich, Switzerland. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Montana, Missoula, MT 59812 USA. LANL, Space & Atmospher Sci, Los Alamos, NM 87544 USA. EM heber@erdw.ethz.ch RI Wieler, Rainer/A-1355-2010; Reisenfeld, Daniel/F-7614-2015 OI Wieler, Rainer/0000-0001-5666-7494; NR 8 TC 1 Z9 1 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A63 EP A63 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800109 ER PT J AU Hutson, ML Ruzicka, AM Mittlefehldt, DW AF Hutson, M. L. Ruzicka, A. M. Mittlefehldt, D. W. TI The case against Mercury as the angrite parent body (APB) SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 Portland State Univ, Cascadia Meteorite Lab, Dept Geol, Portland, OR 97207 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM mhutson@pdx.edu NR 9 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A71 EP A71 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800125 ER PT J AU Ito, M Messenger, S AF Ito, Motoo Messenger, Scott TI Heterogeneous Mg-26 microdistributions in a type A CAI: Constraints on its formation process and chronology SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77573 USA. EM motoo.ito-1@nasa.gov; scott.r.messenger@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A74 EP A74 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800131 ER PT J AU Jones, JH AF Jones, J. H. TI The shergottites are young SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 NASA, JSC, Houston, TX 77058 USA. EM john.h.jones@nasa.gov NR 0 TC 3 Z9 3 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A77 EP A77 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800137 ER PT J AU Keller, LP Messenger, S Walker, RM AF Keller, L. P. Messenger, S. Walker, Robert M. TI Coordinated chemical and isotopic studies of IDPS: Comparison of circumstellar and solar gems grains SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, ARES, Houston, TX 77058 USA. EM Lindsay.P.Keller@nasa.gov NR 4 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A81 EP A81 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800144 ER PT J AU Kita, NT Kimura, M Nyquist, LE AF Kita, N. T. Kimura, M. Nyquist, L. E. TI Microdistribution of oxygen isotopes in chondrules from the least equilibrated H chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 Univ Wisconsin, Madison, WI 53706 USA. Ibaraki Univ, Mito, Ibaraki 3108512, Japan. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM noriko@geology.wisc.edu NR 6 TC 0 Z9 0 U1 0 U2 0 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 AUG PY 2007 VL 42 SU S BP A84 EP A84 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800150 ER PT J AU Kohout, T Kosterov, A Jackson, M Pesonen, LJ Kletetschka, G Lehtinen, M AF Kohout, T. Kosterov, A. Jackson, M. Pesonen, L. J. Kletetschka, G. Lehtinen, M. TI Daubreelite and troilite as a source of cometary and minor body magnetism in cold environment SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 Univ Helsinki, Div Geophys, Helsinki, Finland. Charles Univ Prague, Dept Appl Geophys, Prague, Czech Republic. Acad Sci Czech Republic, Inst Geol, Prague, Czech Republic. Univ Minnesota, Inst Rock Magnetism, Minneapolis, MN USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Univ Helsinki, Geol Museum, Helsinki, Finland. GSFC, NASA, Greenbelt, MD USA. Kochi Univ, Kochi Core Ctr, Nankoku, Kochi, Japan. EM tomas.kohout@helsinki.fi RI Kohout, Tomas/C-1394-2008; Kletetschka, Gunther/C-9996-2011; Kosterov, Andrei/I-4915-2012; Jackson, Mike/G-1587-2013 OI Kohout, Tomas/0000-0003-4458-3650; Kletetschka, Gunther/0000-0002-0645-9037; Kosterov, Andrei/0000-0001-8892-9698; Jackson, Mike/0000-0003-4778-7157 NR 0 TC 1 Z9 1 U1 0 U2 5 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A85 EP A85 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800153 ER PT J AU Kress, ME Tielens, AGGM Frenklach, M AF Kress, M. E. Tielens, A. G. G. M. Frenklach, M. TI The "soot line": Polycyclic aromatic hydrocarbons in primitive chondrites as tracers of nebular conditions SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. NASA, Ames Res Ctr, Div Space Sci, Ames, IA USA. Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. EM mkress@science.sjsu.edu NR 4 TC 0 Z9 0 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A89 EP A89 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800160 ER PT J AU Mabry, JC Meshik, AR Hohenberg, CM Marrocchil, Y Pravdivtseva, OV Allton, J McNamara, K Stansbery, E Burnett, DS AF Mabry, J. C. Meshik, A. R. Hohenberg, C. M. Marrocchil, Y. Pravdivtseva, O. V. Allton, J. McNamara, K. Stansbery, E. Burnett, D. S. TI Solar wind argon from Genesis alos regime collectors SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID NEON; AR C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. NASA, Lyndon B Johnson Space Ctr, Lockheed Martin, Houston, TX 77058 USA. CALTECH, Pasadena, CA 91125 USA. EM jcmabry@wustl.edu NR 7 TC 2 Z9 2 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 AUG PY 2007 VL 42 SU S BP A95 EP A95 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800172 ER PT J AU Martins, Z Alexander, CMO Orzechowska, GE Fogel, ML Sephton, MA Ehrenfreund, P AF Martins, Z. Alexander, C. M. O'D. Orzechowska, G. E. Fogel, M. L. Sephton, M. A. Ehrenfreund, P. TI Indigenous amino acids present in CR primitive meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID ORGANIC-MATTER C1 Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, Impacts & Astromat Res Ctr, London SW7 2AZ, England. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. Leiden Univ, Leiden Inst Chem, Astrobiol Lab, NL-2300 RA Leiden, Netherlands. EM z.martins@chem.leidenuniv.nl NR 4 TC 7 Z9 7 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A97 EP A97 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800177 ER PT J AU Matrajt, G Wirick, S Messenger, S Ito, M Joswiak, D Brownlee, D AF Matrajt, G. Wirick, S. Messenger, S. Ito, M. Joswiak, D. Brownlee, D. TI A TEM, C-XANES, and nanosims investigation of a fragment from the stardust track Ada SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID ORGANIC-MATTER; PARTICLES C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM matrajt@astro.washington.edu NR 7 TC 2 Z9 2 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A99 EP A99 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800180 ER PT J AU Mckay, G Le, L Mikouchi, T AF McKay, G. Le, L. Mikouchi, T. TI Comparison of synthetic and natural nakhlite pyroxenes: Complexity of minor elements SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 NASA, Lyndon B Johnson Space Ctr, ESC Grp, Houston, TX 77058 USA. Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A103 EP A103 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800189 ER PT J AU Meshik, AP Hohenberg, CM Pravdivtseva, OV Mabry, JC Allton, JH McNamara, KM Stansbery, EK Burnett, DS AF Meshik, A. P. Hohenberg, C. M. Pravdivtseva, O. V. Mabry, J. C. Allton, J. H. McNamara, K. M. Stansbery, E. K. Burnett, D. S. TI Preliminary studies of Xe and Kr from the Genesis polished aluminium collector SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. NASA, Lyndon B Johnson Space Ctr, Lockheed Martin, Houston, TX 77058 USA. CALTECH, Pasadena, CA 91125 USA. EM am@physics.wustl.edu NR 1 TC 0 Z9 0 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A105 EP A105 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800192 ER PT J AU Nakamura-Messenger, K Messenger, S Clemett, SJ Keller, LP AF Nakamura-Messenger, K. Messenger, S. Clemett, S. J. Keller, L. P. TI Hydrothermal alteration experiments on anhydrous cometary IDPs SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. NASA, JSC, ESCG, Houston, TX 77058 USA. EM keiko.nakamura-1@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A115 EP A115 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800213 ER PT J AU Park, J Bogard, DD AF Park, Jisun Bogard, Donald D. TI Ar-39-Ar-40 "age" of basaltic shergottite NWA 3171 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID MARTIAN METEORITES; EJECTION TIMES; CHASSIGNY C1 NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. EM jisun.park@nasa.gov NR 9 TC 1 Z9 1 U1 0 U2 4 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A122 EP A122 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800226 ER PT J AU Pearson, VK Morgan, GH Turner, D Perronnet, M Gilmour, I AF Pearson, V. K. Morgan, G. H. Turner, D. Perronnet, M. Gilmour, I. TI Resolution of small-scale structural differences in the CR chondrite macromolecular material SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM v.k.pearson@open.ac.uk NR 7 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A124 EP A124 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800230 ER PT J AU Righter, K AF Righter, K. TI High-pressure, temperature experimental constraints on volatile, siderophile element depletions (Cd, In) in mantles SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID EARLY EARTH; GA; SN C1 NASA, JSC, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A130 EP A130 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800242 ER PT J AU Rotundi, A Baratta, GA Borg, J Brucato, JR Busemann, H Colangeli, L D'Hendecourt, L Djouadi, Z Ferrini, G Franchi, IA Fries, M Grossemy, F Keller, LP Mennella, V Nakamura, K Nittler, LR Palumbo, ME Sandford, SA AF Rotundi, A. Baratta, G. A. Borg, J. Brucato, J. R. Busemann, H. Colangeli, L. D'Hendecourt, L. Djouadi, Z. Ferrini, G. Franchi, I. A. Fries, M. Grossemy, F. Keller, L. P. Mennella, V. Nakamura, K. Nittler, L. R. Palumbo, M. E. Sandford, S. A. TI Combined micro-IR and micro-Raman analyses of comet 81p/wild-2 particles collected by stardust SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 Univ Naples Federico 2, Dip Sci Applicate, I-80138 Naples, Italy. INAF Oss Astr Catania, Catania, Italy. Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. Carnegie Inst, DTM, Washington, DC USA. Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England. Novaetech Srl, Naples, Italy. Carnegie Inst, Washington, DC USA. NASA, JSC, Houston, TX 77058 USA. Jacobs Sverdrup Eng Sci Contract Grp, Houston, TX USA. NASA, Ames Res Ctr, Astroph Branch, Moffett Field, CA 94035 USA. Washington Univ, St Louis, MO 63130 USA. EM rotundi@uniparthenope.it RI Appourchaux, Thierry/F-4692-2010 NR 2 TC 0 Z9 0 U1 1 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A133 EP A133 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800248 ER PT J AU Sandford, SA AF Sandford, S. A. TI "Fixing" interstellar and protosolar D and 'in enrichments into meteoritic materials SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID AMMONIA C1 NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A135 EP A135 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800253 ER PT J AU Sitko, ML Carpenter, KJ Kimes, RL Wilde, JL Lynch, DK Russell, RW Rudy, RJ Mazuk, SM Venturini, CC Puetter, RC Grady, CA Brafford, SM Perry, RB AF Sitko, M. L. Carpenter, K. J. Kimes, R. L. Wilde, J. L. Lynch, D. K. Russell, R. W. Rudy, R. J. Mazuk, S. M. Venturini, C. C. Puetter, R. C. Grady, C. A. Brafford, S. M. Perry, R. B. TI Time variability of the inner dust zone in pre-main sequence disk systems SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. Space Sci Inst, Boulder, CO 80301 USA. Aerosp Corp, Los Angeles, CA 90009 USA. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Eureka Sci Inc, Oakland, CA 94602 USA. Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM sitkoml@ucmail.uc.edu NR 1 TC 0 Z9 0 U1 0 U2 0 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 AUG PY 2007 VL 42 SU S BP A143 EP A143 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800268 ER PT J AU Thomas-Keprta, KL Clemett, SJ McKay, DS Gibson, EK Wentworth, SJ AF Thomas-Keprta, K. L. Clemett, S. J. McKay, D. S. Gibson, E. K. Wentworth, S. J. CA FEI Corporation TI Re-evaluation of the "Life on Mars" hypothesis: Origin of carbonate-magnetite assemblages in Martian meteorite ALH 84001 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID ALH84001; SHOCK C1 NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, KR, ARES, Houston, TX 77058 USA. FEI Co, Hillsboro, OR 97124 USA. EM kthomas@ems.jsc.nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A148 EP A148 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800278 ER PT J AU Velbel, MA Wentworth, SJ Thomas-Keprta, KL Donatelle, AR Mckay, DS AF Velbel, M. A. Wentworth, S. J. Thomas-Keprta, K. L. Donatelle, A. R. Mckay, D. S. TI Microdenticles: Aqueous corrosion textures on weathered chain silicates as terrestrial analogs of pyroxene alteration in mars meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys ID MICHIGAN C1 Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. ESCG, Lyndon B Johnson Space Ctr, Astrobiol Grp, Houston, TX 77058 USA. EM velbel@msu.edu NR 6 TC 0 Z9 0 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A156 EP A156 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800294 ER PT J AU Zolensky, M Ohsumi, K Robinson, G Morgan, G Hagiya, K Mikouchi, T AF Zolensky, Michael Ohsumi, Kazumasa Robinson, GeorgAnn Morgan, Glenn Hagiya, Kenji Mikouchi, Takashi TI Fe-Ni sulfides in chondrites revealed SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 70th Annual Meeting of the Meteoritical-Society CY AUG 13-17, 2007 CL Tucson, AZ SP Meteorit Soc, Univ Arizona Lunar & Planetary Lab, Univ Arizona Dept Geosci, Univ Arizona Coll Sci, Life & Planets Astrobiol Ctr, NSF Arizona AMS Lab, SW Meteorite Ctr, Steward Observ, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, Planetary Sci Inst, Barringer Crater Co, Lockheed Martin, Cameca, New Wave, Planetary Studies Fdn, Thermo Finnigan, Univ Arizona Press, Tucson Visitors & Convent Bur, Univ Arizona Dept Phys C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Jacobs Sverdrup, Houston, TX 77058 USA. Jacobs Engn, Houston, TX 77058 USA. Hyogo Univ, Hyogo 6781297, Japan. Univ Tokyo, Tokyo 1130033, Japan. EM michael.e.zolensky@nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2007 VL 42 SU S BP A171 EP A171 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 200HZ UT WOS:000248755800324 ER PT J AU Jinka, KK Ganesan, S Dasgupta, A Ling, S Shapiro, A Schatzel, D AF Jinka, K. K. Ganesan, S. Dasgupta, A. Ling, S. Shapiro, A. Schatzel, D. TI Chip-on-Board (CoB) technology for low temperature environments. Part I: Wire profile modeling in unencapsulated chips SO MICROELECTRONICS RELIABILITY LA English DT Article AB An analytical model based on elastic strain energy minimization is developed for estimating the wire profile in unencapsulated ball wedge wire bond configuration for chip-on-board (CoB) technology. The wire profile is applicable to ball-wedge bonds with a height Off-set, and is modeled using a piece-wise continuous polynomial function (cubic spline) with appropriate boundary conditions at the two bond sites. Plastic deformation is ignored in the current analysis as a first-order approximation, since the interest is in parametric sensitivity studies. The model is useful for estimating the wire profile for different offset heights and wire spans, and serves as a starting point for subsequent thermornechanical stress analysis after encapsulation. Parametric studies are presented to explore the wire profile for different CoB geometries. (c) 2006 Elsevier Ltd. All rights reserved. C1 Univ Maryland, CALCE Elect Prod & Syst Ctr, College Pk, MD 20742 USA. Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA. NASA, Jet Propuls Lab, Pasadena, CA 91109 USA. RP Jinka, KK (reprint author), Univ Maryland, CALCE Elect Prod & Syst Ctr, College Pk, MD 20742 USA. EM krishna9780@gmail.com; dasgupta@umd.edu NR 6 TC 4 Z9 5 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0026-2714 J9 MICROELECTRON RELIAB JI Microelectron. Reliab. PD AUG PY 2007 VL 47 IS 8 BP 1246 EP 1250 DI 10.1016/j.microrel.2006.08.019 PG 5 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA 205AZ UT WOS:000249086500016 ER PT J AU Rodgers, SD Charnley, SB Smith, RG Butner, HM AF Rodgers, S. D. Charnley, S. B. Smith, R. G. Butner, H. M. TI Chemical chronology of the Southern Coalsack SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; molecular processes; ISM : clouds; ISM : individual : Coalsack; ISM : molecules ID INFRARED IMAGING SURVEY; STAR-FORMATION; MOLECULAR CLOUDS; DARK CLOUDS; INTERSTELLAR CLOUDS; BOK GLOBULES; HOT CORES; ICE; CHEMISTRY; ABUNDANCES AB We demonstrate how the observed H2O ice column densities toward three dense globules in the Southern Coalsack could be used to constrain the ages of these sources. We derive ages of similar to 10(5) yr, in agreement with dynamical studies of these objects. We have modelled the chemical evolution of the globules and showed how the molecular abundances are controlled by both the gas density and the initial chemical conditions as the globules formed. Based on our derived ages, we predict the column densities of several species of interest. These predictions should be straightforward to test by performing molecular-line observations. C1 NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. Univ New S Wales, Sch Phys Environm & Math Sci, Australian Def Force Acad, Canberra, ACT 2600, Australia. James Madison Univ, Dept Phys, Harrisonburg, VA 22807 USA. RP Rodgers, SD (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM rodgers@dusty.arc.nasa.gov RI Charnley, Steven/C-9538-2012; OI Butner, Harold/0000-0003-4899-2064 NR 50 TC 1 Z9 1 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2007 VL 379 IS 2 BP 807 EP 815 DI 10.1111/j.1365-2966.2007.11985.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 209GN UT WOS:000249377100028 ER PT J AU Lin, X Zhang, SQ Hou, AY AF Lin, Xin Zhang, Sara Q. Hou, Arthur Y. TI Variational assimilation of global microwave rainfall retrievals: Physical and dynamical impact on GEOS analyses SO MONTHLY WEATHER REVIEW LA English DT Article ID RADIATION BUDGET EXPERIMENT; ENERGY SYSTEM CERES; PACIFIC WARM POOL; PRECIPITATION DATA; 1D+4D-VAR ASSIMILATION; MOISTURE OBSERVATIONS; 4D-VAR ASSIMILATION; HUMIDITY PROFILES; MESOSCALE MODEL; TMI RAINFALL AB Global microwave rainfall retrievals from a five- satellite constellation, including the Tropical Rainfall Measuring Mission Microwave Imager, Special Sensor Microwave Imager from the Defense Meteorological Satellite Program F13, F14, and F15, and the Advanced Microwave Scanning Radiometer from the Earth Observing System Aqua, are assimilated into the NASA Goddard Earth Observing System ( GEOS) Data Assimilation System using a 1D variational continuous assimilation ( VCA) algorithm. The physical and dynamical impact of rainfall assimilation on GEOS analyses is examined at various temporal and spatial scales. This study demonstrates that the 1D VCA algorithm, which was originally developed and evaluated for rainfall assimilations over tropical oceans, can effectively assimilate satellite microwave rainfall retrievals and improve GEOS analyses over both the Tropics and the extratropics where the atmospheric processes are dominated by different large- scale dynamics and moist physics, and also over land, where rainfall estimates from passive microwave radiometers are believed to be less accurate. Results show that rainfall assimilation renders the GEOS analysis physically and dynamically more consistent with the observed precipitation at the monthly mean and 6- h time scales. Over regions where the model precipitation tends to misbehave in distinctly different rainy regimes, the 1D VCA algorithm, by compensating for errors in the model's moist time tendency in a 6- h analysis window, is able to bring the rainfall analysis closer to the observed. The radiation and cloud fields also tend to be in better agreement with independent satellite observations in the rainfall - assimilation run especially over regions where rainfall analyses indicate large improvements. Assimilation experiments with and without rainfall data for a midlatitude frontal system clearly indicate that the GEOS analysis is improved through changes in the thermodynamic and dynamic fields that respond to the rainfall assimilation. The synoptic structures of temperature, moisture, winds, divergence, and vertical motion, as well as vorticity, are more realistically captured across the front. C1 NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD USA. Sci Applicat Int Corp, Beltsville, MD USA. RP Lin, X (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 660-1, Greenbelt, MD 20771 USA. EM xlin@gmao.gsfc.nasa.gov RI Hou, Arthur/D-8578-2012 NR 49 TC 4 Z9 4 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD AUG PY 2007 VL 135 IS 8 BP 2931 EP 2957 DI 10.1175/MWR3434.1 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 199WV UT WOS:000248726800008 ER PT J AU Verzani, CJ Miller, K Wrigley, A Kessel, Q Smith, WW Smith, SJ Hossain, S Chutjian, A AF Verzani, C. J. Miller, K. Wrigley, A. Kessel, Q. Smith, W. W. Smith, S. J. Hossain, S. Chutjian, A. TI Laboratory measurements of 50-300 eV X rays from collisions of cometary interest: Ne and S L X rays, Fe M X rays and others SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 19th International Conference on Application of Accelerators in Research and Industry CY AUG 20-25, 2006 CL Ft Worth, TX SP Lawrence Berkeley Natl Lab, Lawrence Livemore Natl Lab, Los Alamos Natl Lab, Natl Canc Inst, Oak Ridge Associated Univ, Oak Ridge Natl Lab, Sandia Natl Lab, Univ N Texas, AccSys Technol Inc, Comecer SRL, Natl Electrostat Corp, Synergy Vacuum DE electron capture; solar wind; comets ID ELECTRON-CAPTURE; EMISSION; ATOMS; IONS AB Laboratory measurements simulating the impact of certain solar wind ions on CO have been made. Preliminary analysis of the X rays in the 50-300 eV energy range produced by these collisions suggests that a dominant role is played by electron capture and subsequent relaxation of the electron to the n = 2 levels of solar wind ions such as Ne and S. In particular our data show that X rays from Ne play a role that is at least as significant as that of the more dominant solar wind ion O6+ in this X-ray energy range. It may be assumed that Mg and Si may also play an important role; however, these ions were not included in the present experiment. (c) 2007 Elsevier B.V. All rights reserved. C1 Univ Connecticut, Inst Mat Sci, Dept Phys, Unit 3046, Storrs, CT 06268 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kessel, Q (reprint author), Univ Connecticut, Inst Mat Sci, Dept Phys, Unit 3046, Storrs, CT 06268 USA. EM quentin.kessel@uconn.edu NR 11 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD AUG PY 2007 VL 261 IS 1-2 BP 189 EP 192 DI 10.1016/j.nimb.2007.04.012 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 200SW UT WOS:000248784100048 ER PT J AU Tanis, JA Hossain, S AF Tanis, J. A. Hossain, S. TI Electron interferences in the ionization of H-2 SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 19th International Conference on Application of Accelerators in Research and Industry CY AUG 20-25, 2006 CL Ft Worth, TX SP Lawrence Berkeley Natl Lab, Lawrence Livemore Natl Lab, Los Alamos Natl Lab, Natl Canc Inst, Oak Ridge Associated Univ, Oak Ridge Natl Lab, Sandia Natl Lab, Univ N Texas, AccSys Technol Inc, Comecer SRL, Natl Electrostat Corp, Synergy Vacuum DE electron interferences; ionization; two-center emission ID ION IMPACT; EMISSION AB Oscillatory structures observed in the velocity distributions of the ejected electron spectra from H, impacted by fast H+ (v/c similar to 0.1) and Kr34+ (v/c similar to 0.3) ions are reviewed. In addition to the primary Young-type electron interferences, secondary interferences due to intramolecular scattering, as well as considerably higher-frequency oscillations of as yet unknown origin, are observed. Dependences of the oscillations on the electron observation angle and collision velocity are discussed and compared with theory. (c) 2007 Elsevier B.V. All rights reserved. C1 Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tanis, JA (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. EM john.tanis@wmich.edu NR 25 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD AUG PY 2007 VL 261 IS 1-2 BP 226 EP 229 DI 10.1016/j.nimb.2007.04.266 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 200SW UT WOS:000248784100058 ER PT J AU Refaat, TF Ismail, S Mack, TL Abedin, MN Mayor, SD Spuler, SM Singh, UN AF Refaat, Tamer F. Ismail, Syed Mack, Terry L. Abedin, M. Nurul Mayor, Shane D. Spuler, Scott M. Singh, Upendra N. TI Infrared phototransistor validation for atmospheric remote sensing application using the Raman-shifted eye-safe aerosol lidar SO OPTICAL ENGINEERING LA English DT Article DE phototransistor; InGaAsSb; remote sensing; lidar; carbon dioxide ID ALGAASSB/INGAASSB PHOTOTRANSISTORS; SENSITIVITY ANALYSIS; WATER-VAPOR; MU-M; RANGE AB An InGaAsSb/AlGaAsSb phototransistor has been validated for lidar atmospheric remote sensing. The validation was performed using the Raman-shifted eye-safe aerosol lidar (REAL) at the National Center for Atmospheric Research. Although the device is optimized for detection around the 2-mu m wavelength, the validation was performed at 1.543 mu m, where mature commercial detectors are available. Simultaneous measurement of the atmospheric backscatter signals using the custom-built phototransistor and commercial InGaAs avalanche photodiode indicated good agreement between both devices. The validation included detecting 11-km-range hard targets, 5-km atmospheric structure consisting of cirrus clouds, and a near-field boundary layer. Far-field low intensity and spatially narrow atmospheric features were also detectable with the new phototransistor. Preliminary results related to systematic effects are discussed in the first attempt of incorporating a phototransistor in a lidar system. (c) 2007 Society of Photo-Optical Instrumentation Engineers. C1 Old Dominion Univ, Appl Res Ctr, Newport News, VA 23606 USA. NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Pass sensor Syst Branch, Hampton, VA 23681 USA. Natl Ctr Atmospher Res, Div Atmospher Technol, Boulder, CO 80307 USA. NASA, Langley Res Ctr, Syst Engn Directorate, Hampton, VA 23681 USA. RP Refaat, TF (reprint author), Old Dominion Univ, Appl Res Ctr, 12050 Jefferson Ave, Newport News, VA 23606 USA. NR 19 TC 5 Z9 5 U1 0 U2 2 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD AUG PY 2007 VL 46 IS 8 AR 086001 DI 10.1117/1.2772280 PG 8 WC Optics SC Optics GA 221BB UT WOS:000250200800026 ER PT J AU Stephen, M Krainak, M Riris, H Allan, GR AF Stephen, Mark Krainak, Michael Riris, Haris Allan, Graham R. TI Narrowband, tunable, frequency-doubled, erbium-doped fiber-amplifed transmitter SO OPTICS LETTERS LA English DT Article ID DIFFERENTIAL ABSORPTION LIDAR; ATMOSPHERIC-PRESSURE; LASER SOURCE; NM AB We report on the development of a fiber-based laser transmitter designed for active remote sensing spectroscopy. The transmitter uses a master oscillator power amplifier (MOPA) configuration with a distributed feedback diode-laser master oscillator and an erbium-doped fiber amplifier. The output from the MOPA is frequency-doubled with a periodically poled potassium titanium oxide phosphate crystal. With 35 W of single-frequency peak optical pump power, 8 W of frequency-doubled peak power was achieved. The utility of this single-frequency, wavelength tunable, power scalable laser was then demonstrated in a spectroscopic measurement of diatomic oxygen A band. (C) 2007 Optical Society of America. C1 NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Greenbelt, MD 20771 USA. Sigma Space Corp, Lanham, MD 20706 USA. RP Stephen, M (reprint author), NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Code 661, Greenbelt, MD 20771 USA. EM mark.a.stephen@nasa.gov RI Riris, Haris/D-1004-2013; Allan, Graham/D-3905-2013 NR 14 TC 21 Z9 21 U1 5 U2 11 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD AUG 1 PY 2007 VL 32 IS 15 BP 2073 EP 2075 DI 10.1364/OL.32.002073 PG 3 WC Optics SC Optics GA 205BF UT WOS:000249087200001 PM 17671540 ER PT J AU Savchenkov, AA Matsko, AB Ilchenko, VS Strekalov, D Maleki, L AF Savchenkov, A. A. Matsko, A. B. Ilchenko, V. S. Strekalov, D. Maleki, L. TI Direct observation of stopped light in a whispering-gallery-mode microresonator SO PHYSICAL REVIEW A LA English DT Article ID ATOMIC GAS; STORAGE AB We introduce the definition of group velocity for a system with a discrete spectrum and apply it to a linear resonator. We show that a positive, negative, or zero group velocity can be obtained for light propagating in the whispering-gallery modes of a microspherical resonator. The associated group delay is practically independent of the ring-down time of the resonator. We demonstrate "stopped light" in an experiment with a fused silica microsphere. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Savchenkov, AA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Matsko, Andrey/A-1272-2007 NR 8 TC 28 Z9 28 U1 6 U2 13 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD AUG PY 2007 VL 76 IS 2 AR 023816 DI 10.1103/PhysRevA.76.023816 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 205ZY UT WOS:000249154900144 ER PT J AU Bakunov, MI Bodrov, SB Maslov, AV Hangyo, M AF Bakunov, M. I. Bodrov, S. B. Maslov, A. V. Hangyo, M. TI Theory of terahertz generation in a slab of electro-optic material using an ultrashort laser pulse focused to a line SO PHYSICAL REVIEW B LA English DT Article ID FEMTOSECOND OPTICAL PULSES; POLED LITHIUM-NIOBATE; CHERENKOV RADIATION; EFFICIENT GENERATION; DIRECT VISUALIZATION; THZ RADIATION; FIBER LASER; RECTIFICATION; CRYSTALS; AREA AB A theory that describes the optical-to-terahertz conversion of femtosecond laser pulses via optical rectification in a slab of an electro-optic material is developed. Two typical experimental situations-phase-matched regime (ZnTe excited with 780 nm optical pump) and non-phase-matched regime (LiNbO3 excited with 800 nm optical pump and GaAs excited with 1.56 mu m optical pump)-are considered. The theory accounts for the transverse size of the laser beam and allows us to explore the dependence of the conversion efficiency on laser focusing. We trace the temporal dynamics of the optical-to-terahertz conversion inside the slab and study the angular distribution of the terahertz emission from the slab. The optimal parameters (such as laser transverse size and crystal thickness) maximizing the terahertz yield for ZnTe and GaAs are calculated. C1 Univ Nizhny Novgorod, Dept Radiophys, Nizhnii Novgorod 603950, Russia. Russian Acad Sci, Inst Phys Appl, Nizhnii Novgorod 603950, Russia. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Osaka Univ, Inst Laser Engn, Laser Terahertz Div, Suita, Osaka 5650871, Japan. RP Bakunov, MI (reprint author), Canon Dev Americas Inc, Irvine, CA USA. RI Maslov, Alexey/E-5158-2011; Bodrov, Sergey/D-1962-2012; Bakunov, Michael/E-2875-2017 OI Maslov, Alexey/0000-0002-7835-2474; Bakunov, Michael/0000-0002-4209-1372 NR 46 TC 38 Z9 38 U1 0 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD AUG PY 2007 VL 76 IS 8 AR 085346 DI 10.1103/PhysRevB.76.085346 PG 18 WC Physics, Condensed Matter SC Physics GA 206AD UT WOS:000249155400098 ER PT J AU Palmer, BS Sanchez, CA Naik, A Manheimer, MA Schneiderman, JF Echternach, PM Wellstood, FC AF Palmer, B. S. Sanchez, C. A. Naik, A. Manheimer, M. A. Schneiderman, J. F. Echternach, P. M. Wellstood, F. C. TI Steady-state thermodynamics of nonequilibrium quasiparticles in a Cooper-pair box SO PHYSICAL REVIEW B LA English DT Article ID TRANSISTOR; JUNCTIONS; QUBIT AB A superconducting Coulomb-blockade electrometer was used to measure the Coulomb staircase of an Al/AlOx/Al Cooper-pair box from a temperature of 30 to 300 mK. At the lowest temperature, the Coulomb staircase displays effects from nonequilibrium quasiparticles. As the temperature is increased, an initial decrease is found in the width of the odd steps in the staircase, which corresponds to a reduction in the probability of having a quasiparticle on the island of the box. Above 180 mK, the width of the odd steps increases, eventually producing a staircase with 1e features. We develop a steady-state model of the system and find that the presence of quasiparticles at low temperature is consistent with the assumption of Aumentado [Phys. Rev. Lett. 92, 066802 (2004)] that nonequilibrium quasiparticles are generated in the leads. Above 180 mK, our results are consistent with the quasiparticle states of the island being thermally populated. C1 Lab Phys Sci, College Pk, MD 20740 USA. Univ So Calif, Dept Phys, Los Angeles, CA 90089 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Maryland, Ctr Supercond Res, College Pk, MD 20742 USA. Univ Maryland, Dept Phys, Joint Quantum Inst, College Pk, MD 20742 USA. RP Palmer, BS (reprint author), Lab Phys Sci, College Pk, MD 20740 USA. EM bpalmer@lps.umd.edu RI naik, akshay/C-4108-2009; Joint Quantum Institute, NIST/UMD/H-4494-2011; Manheimer, Marc/D-6320-2013; Schneiderman, Justin/D-4508-2013 OI naik, akshay/0000-0001-6325-7231; Schneiderman, Justin/0000-0002-4441-2360 NR 21 TC 14 Z9 14 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD AUG PY 2007 VL 76 IS 5 AR 054501 DI 10.1103/PhysRevB.76.054501 PG 7 WC Physics, Condensed Matter SC Physics GA 206AA UT WOS:000249155100125 ER PT J AU Abbott, B Abbott, R Adhikari, R Agresti, J Ajith, P Allen, B Amin, R Anderson, SB Anderson, WG Arain, M Araya, M Armandula, H Ashley, M Aston, S Aufmuth, P Aulbert, C Babak, S Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barton, MA Bayer, K Belczynski, K Betzwieser, J Beyersdorf, PT Bhawal, B Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, K Blackburn, L Blair, D Bland, B Bogenstahl, J Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, A Brown, DA Bullington, A Bunkowski, A Buonanno, A Burmeister, O Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cao, J Cardenas, L Carter, K Casey, MM Castaldi, G Cepeda, C Chalkey, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Chiadini, F Chin, D Chin, E Chow, J Christensen, N Clark, J Cochrane, P Cokelaer, T Colacino, CN Coldwell, R Conte, R Cook, D Corbitt, T Coward, D Coyne, D Creighton, JDE Creighton, TD Croce, RP Crooks, DRM Cruise, AM Cumming, A Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Debra, D Degallaix, J Degree, M Demma, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dickson, J Di Credico, A Diederichs, G Dietz, A Doomes, EE Drever, RWP Dumas, JC Dupuis, RJ Dwyer, JG Ehrens, P Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Fan, Y Fazi, D Fejer, MM Finn, LS Fiumara, V Fotopoulos, N Franzen, A Franzen, KY Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Ganezer, KS Garofoli, J Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, L Gonzalez, G Gossler, S Grant, A Gras, S Gray, C Gray, M Greenhalgh, J Gretarsson, AM Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, R Hage, B Hammer, D Hanna, C Hanson, J Harms, J Harry, G Harstad, E Hayler, T Heefner, J Heng, IS Heptonstall, A Heurs, M Hewitson, M Hild, S Hirose, E Hoak, D Hosken, D Hough, J Howell, E Hoyland, D Huttner, SH Ingram, D Innerhofer, E Ito, M Itoh, Y Ivanov, A Jackrel, D Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalili, FY Kim, C King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, RK Kozak, D Krishnan, B Kwee, P Lam, PK Landry, M Lantz, B Lazzarini, A Lee, B Lei, M Leiner, J Leonhardt, V Leonor, I Libbrecht, K Lindquist, P Lockerbie, NA Longo, M Lormand, M Lubinski, M Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Malec, M Mandic, V Marano, S Marka, S Markowitz, J Maros, E Martin, I Marx, JN Mason, K Matone, L Matta, V Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McKenzie, K McNabb, JWC McWilliams, S Meier, T Melissinos, A Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, CJ Meyers, D Mikhailov, E Mitra, S Mitrofanov, P Mitselmakher, G Mittleman, R Miyakawa, O Mohanty, S Moreno, G Mossavi, K MowLowry, C Moylan, A Mudge, D Mueller, G Mukherjee, S Mueller-Ebhardt, H Munch, J Murray, P Myers, E Myers, J Nash, T Newton, G Nishizawa, A Nocera, F Numata, K O'Reilly, B O'Shaughnessy, R Ottaway, DJ Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Parameswariah, C Patel, P Pedraza, M Penn, S Pierro, V Pinto, IM Pitkin, M Pletsch, H Plissi, MV Postiglione, F Prix, R Quetschke, V Raab, F Rabeling, D Radkins, H Rahkola, R Rainer, N Rakhmanov, M Rawlins, K Ray-Majumder, S Re, V Regimbau, T Rehbein, H Reid, S Reitze, DH Ribichini, L Riesen, R Riles, K Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rodriguez, A Rogan, AM Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rodriguez, A Rogan, AM Rollins, J Romano, JD Romie, J Route, R Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Sakata, S Samidi, M de la Jordana, LS Sandberg, V Sanders, GH Sannibale, V Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P Sazonov, A Schediwy, S Schilling, R Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Shawhan, P Shoemaker, DH Sibley, A Sidles, JA Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Somiya, K Strain, KA Strom, DM Stuver, A Summerscales, TZ Sun, KX Sung, M Sutton, PJ Takahashi, H Tanner, DB Tarallo, M Taylor, R Taylor, R Thacker, J Thorne, KA Thorne, KS Thuring, A Tokmakov, V Torres, C Torrie, C Traylor, G Trias, M Tyler, W Ugolini, D Ungarelli, C Urbanek, K Vahlbruch, H Vallisneri, M Van den Broeck, C van Putten, M Varvella, M Vass, S Vecchio, A Veitch, J Veitch, P Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, R Watts, K Webber, D Weidner, A Weinert, M Weinstein, A Weiss, R Wen, S Wette, K Whelan, JT Whitbeck, DM Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Yunes, N Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, M zur Muehlen, H Zweizig, J Kramer, M Lyne, AG AF Abbott, B. Abbott, R. Adhikari, R. Agresti, J. Ajith, P. Allen, B. Amin, R. Anderson, S. B. Anderson, W. G. Arain, M. Araya, M. Armandula, H. Ashley, M. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Ballmer, S. Bantilan, H. Barish, B. C. Barker, C. Barker, D. Barr, B. Barriga, P. Barton, M. A. Bayer, K. Belczynski, K. Betzwieser, J. Beyersdorf, P. T. Bhawal, B. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, K. Blackburn, L. Blair, D. Bland, B. Bogenstahl, J. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brooks, A. Brown, D. A. Bullington, A. Bunkowski, A. Buonanno, A. Burmeister, O. Busby, D. Butler, W. E. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. Cantley, C. A. Cao, J. Cardenas, L. Carter, K. Casey, M. M. Castaldi, G. Cepeda, C. Chalkey, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Chiadini, F. Chin, D. Chin, E. Chow, J. Christensen, N. Clark, J. Cochrane, P. Cokelaer, T. Colacino, C. N. Coldwell, R. Conte, R. Cook, D. Corbitt, T. Coward, D. Coyne, D. Creighton, J. D. E. Creighton, T. D. Croce, R. P. Crooks, D. R. M. Cruise, A. M. Cumming, A. Dalrymple, J. D'Ambrosio, E. Danzmann, K. Davies, G. DeBra, D. Degallaix, J. Degree, M. Demma, T. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dickson, J. Di Credico, A. Diederichs, G. Dietz, A. Doomes, E. E. Drever, R. W. P. Dumas, J.-C. Dupuis, R. J. Dwyer, J. G. Ehrens, P. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Fan, Y. Fazi, D. Fejer, M. M. Finn, L. S. Fiumara, V. Fotopoulos, N. Franzen, A. Franzen, K. Y. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Ganezer, K. S. Garofoli, J. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. Gonzalez, G. Gossler, S. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, J. Gretarsson, A. M. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, R. Hage, B. Hammer, D. Hanna, C. Hanson, J. Harms, J. Harry, G. Harstad, E. Hayler, T. Heefner, J. Heng, I. S. Heptonstall, A. Heurs, M. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hosken, D. Hough, J. Howell, E. Hoyland, D. Huttner, S. H. Ingram, D. Innerhofer, E. Ito, M. Itoh, Y. Ivanov, A. Jackrel, D. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalili, F. Ya. Kim, C. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. K. Kozak, D. Krishnan, B. Kwee, P. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lee, B. Lei, M. Leiner, J. Leonhardt, V. Leonor, I. Libbrecht, K. Lindquist, P. Lockerbie, N. A. Longo, M. Lormand, M. Lubinski, M. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Malec, M. Mandic, V. Marano, S. Marka, S. Markowitz, J. Maros, E. Martin, I. Marx, J. N. Mason, K. Matone, L. Matta, V. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McKenzie, K. McNabb, J. W. C. McWilliams, S. Meier, T. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messaritaki, E. Messenger, C. J. Meyers, D. Mikhailov, E. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Mohanty, S. Moreno, G. Mossavi, K. MowLowry, C. Moylan, A. Mudge, D. Mueller, G. Mukherjee, S. Mueller-Ebhardt, H. Munch, J. Murray, P. Myers, E. Myers, J. Nash, T. Newton, G. Nishizawa, A. Nocera, F. Numata, K. O'Reilly, B. O'Shaughnessy, R. Ottaway, D. J. Overmier, H. Owen, B. J. Pan, Y. Papa, M. A. Parameshwaraiah, V. Parameswariah, C. Patel, P. Pedraza, M. Penn, S. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. Plissi, M. V. Postiglione, F. Prix, R. Quetschke, V. Raab, F. Rabeling, D. Radkins, H. Rahkola, R. Rainer, N. Rakhmanov, M. Rawlins, K. Ray-Majumder, S. Re, V. Regimbau, T. Rehbein, H. Reid, S. Reitze, D. H. Ribichini, L. Riesen, R. Riles, K. Rivera, B. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rodriguez, A. Rogan, A. M. Rivera, B. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rodriguez, A. Rogan, A. M. Rollins, J. Romano, J. D. Romie, J. Route, R. Rowan, S. Ruediger, A. Ruet, L. Russell, P. Ryan, K. Sakata, S. Samidi, M. de la Jordana, L. Sancho Sandberg, V. Sanders, G. H. Sannibale, V. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Saulson, P. R. Savage, R. Savov, P. Sazonov, A. Schediwy, S. Schilling, R. Schnabel, R. Schofield, R. Schutz, B. F. Schwinberg, P. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Shawhan, P. Shoemaker, D. H. Sibley, A. Sidles, J. A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Somiya, K. Strain, K. A. Strom, D. M. Stuver, A. Summerscales, T. Z. Sun, K.-X. Sung, M. Sutton, P. J. Takahashi, H. Tanner, D. B. Tarallo, M. Taylor, R. Taylor, R. Thacker, J. Thorne, K. A. Thorne, K. S. Thuering, A. Tokmakov, V. Torres, C. Torrie, C. Traylor, G. Trias, M. Tyler, W. Ugolini, D. Ungarelli, C. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van den Broeck, C. van Putten, M. Varvella, M. Vass, S. Vecchio, A. Veitch, J. Veitch, P. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, H. Ward, R. Watts, K. Webber, D. Weidner, A. Weinert, M. Weinstein, A. Weiss, R. Wen, S. Wette, K. Whelan, J. T. Whitbeck, D. M. Whitcomb, S. E. Whiting, B. F. Wiley, S. Wilkinson, C. Willems, P. A. Williams, L. Willke, B. Wilmut, I. Winkler, W. Wipf, C. C. Wise, S. Wiseman, A. G. Woan, G. Woods, D. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Yunes, N. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. zur Muehlen, H. Zweizig, J. Kramer, M. Lyne, G. TI Upper limits on gravitational wave emission from 78 radio pulsars SO PHYSICAL REVIEW D LA English DT Article ID EQUATION-OF-STATE; TIMING NOISE; CRAB PULSAR; NEUTRON; INERTIA; RADIATION; MOMENT; TELESCOPE; GEO-600; MODELS AB We present upper limits on the gravitational wave emission from 78 radio pulsars based on data from the third and fourth science runs of the LIGO and GEO 600 gravitational wave detectors. The data from both runs have been combined coherently to maximize sensitivity. For the first time, pulsars within binary (or multiple) systems have been included in the search by taking into account the signal modulation due to their orbits. Our upper limits are therefore the first measured for 56 of these pulsars. For the remaining 22, our results improve on previous upper limits by up to a factor of 10. For example, our tightest upper limit on the gravitational strain is 2.6x10(-25) for PSR J1603-7202, and the equatorial ellipticity of PSR J2124-3358 is less than 10(-6). Furthermore, our strain upper limit for the Crab pulsar is only 2.2 times greater than the fiducial spin-down limit. C1 Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. Andrews Univ, Berrien Springs, MI 49104 USA. Australian Natl Univ, Canberra, ACT 0200, Australia. CALTECH, Pasadena, CA 91125 USA. Calif State Univ Dominguez Hills, Carson, CA 90747 USA. CALTECH, CaRT, Pasadena, CA 91125 USA. Cardiff Univ, Cardiff CF2 3YB, S Glam, Wales. Carleton Coll, Northfield, MN 55057 USA. Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. Columbia Univ, New York, NY 10027 USA. Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. Hobart & William Smith Coll, Geneva, NY 14456 USA. Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. CALTECH, LIGO, Pasadena, CA 91125 USA. LIGO Hanford Observ, Richland, WA 99352 USA. LIGO Livingston Observ, Livingston, LA 70754 USA. MIT, LIGO, Cambridge, MA 02139 USA. Louisiana State Univ, Baton Rouge, LA 70803 USA. Louisiana Tech Univ, Ruston, LA 71272 USA. Loyola Univ, New Orleans, LA 70118 USA. Moscow MV Lomonosov State Univ, Moscow 119992, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Astron Observ, Tokyo 1818588, Japan. Northwestern Univ, Evanston, IL 60208 USA. Rochester Inst Technol, Rochester, NY 14623 USA. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. San Jose State Univ, San Jose, CA 95192 USA. SE Louisiana Univ, Hammond, LA 70402 USA. So Univ, Baton Rouge, LA 70813 USA. A&M Coll, Baton Rouge, LA 70813 USA. Stanford Univ, Stanford, CA 94305 USA. Syracuse Univ, Syracuse, NY 13244 USA. Penn State Univ, University Pk, PA 16802 USA. Univ Texas, Brownsville, TX 78520 USA. Texas S Most Coll, Brownsville, TX 78520 USA. Trinity Univ, San Antonio, TX 78212 USA. Univ Illes Balears, E-07122 Palma de Mallorca, Spain. Leibniz Univ Hannover, D-30167 Hannover, Germany. Univ Adelaide, Adelaide, SA 5005, Australia. Univ Birmingham, Birmingham B15 2TT, W Midlands, England. Univ Florida, Gainesville, FL 32611 USA. Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. Univ Maryland, College Pk, MD 20742 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Univ Oregon, Eugene, OR 97403 USA. Univ Rochester, Rochester, NY 14627 USA. Univ Salerno, I-84084 Salerno, Italy. Univ Sannio Benevento, I-82100 Benevento, Italy. Univ Southampton, Southampton SO17 1BJ, Hants, England. Univ Strathclyde, Glasgow G1 1WQ, Lanark, Scotland. Univ Washington, Seattle, WA 98195 USA. Univ Western Australia, Crawley, Washington 6009, Australia. Univ Wisconsin, Milwaukee, WI 53201 USA. Vassar Coll, New York, NY 12604 USA. Washington State Univ, Pullman, WA 99164 USA. RP Pitkin, M (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. EM matthew@astro.gla.ac.uk RI Frey, Raymond/E-2830-2016; Howell, Eric/H-5072-2014; Ward, Robert/I-8032-2014; van Putten, Maurice/F-5237-2011; Khalili, Farit/D-8113-2012; Chiadini, Francesco/E-1812-2015; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Messaritaki, Eirini/D-7393-2016; Tarallo, Marco/B-2096-2012; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Chow, Jong/A-3183-2008; Agresti, Juri/G-8168-2012; Ju, Li/C-2623-2013; Barker, David/A-5671-2013; Lueck, Harald/F-7100-2011; Kawabe, Keita/G-9840-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Galdi, Vincenzo/B-1670-2008; Barriga, Pablo/A-3929-2008; zhao, chunnong/A-1373-2008; Lam, Ping Koy/A-5276-2008; Finn, Lee Samuel/A-3452-2009; Vyatchanin, Sergey/J-2238-2012; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010; McClelland, David/E-6765-2010; Pitkin, Matthew/I-3802-2013; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Casey, Morag/C-9703-2010; Chen, Yanbei/A-2604-2013; Allen, Bruce/K-2327-2012; Bilenko, Igor/D-5172-2012; Mitrofanov, Valery/D-8501-2012 OI Freise, Andreas/0000-0001-6586-9901; MATTA, VINCENZO/0000-0002-2046-4027; MARANO, Stefano/0000-0002-5307-0980; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Papa, M.Alessandra/0000-0002-1007-5298; Stuver, Amber/0000-0003-0324-5735; Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Aulbert, Carsten/0000-0002-1481-8319; Frey, Raymond/0000-0003-0341-2636; Howell, Eric/0000-0001-7891-2817; LONGO, Maurizio/0000-0001-8325-4003; Pierro, Vincenzo/0000-0002-6020-5521; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Pinto, Innocenzo M./0000-0002-2679-4457; Chiadini, Francesco/0000-0002-9339-8622; Vecchio, Alberto/0000-0002-6254-1617; Postiglione, Fabio/0000-0003-0628-3796; Tarallo, Marco/0000-0001-5169-4987; Sigg, Daniel/0000-0003-4606-6526; Chow, Jong/0000-0002-2414-5402; Agresti, Juri/0000-0001-6119-2470; Lueck, Harald/0000-0001-9350-4846; Galdi, Vincenzo/0000-0002-4796-3600; Lam, Ping Koy/0000-0002-4421-601X; Finn, Lee Samuel/0000-0002-3937-0688; McClelland, David/0000-0001-6210-5842; Pitkin, Matthew/0000-0003-4548-526X; Strain, Kenneth/0000-0002-2066-5355; Allen, Bruce/0000-0003-4285-6256; NR 51 TC 96 Z9 96 U1 2 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD AUG PY 2007 VL 76 IS 4 AR 042001 DI 10.1103/PhysRevD.76.042001 PG 20 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 206AH UT WOS:000249155800009 ER PT J AU Birn, J Hesse, M AF Birn, J. Hesse, M. TI Reconnection rates in driven magnetic reconnection SO PHYSICS OF PLASMAS LA English DT Article ID COALESCENCE INSTABILITY; CURRENT SHEETS; ISLANDS; MAGNETOTAIL; CHALLENGE; FIELDS AB Using resistive magnetohydrodynamic simulations, we investigate the influence of various parameters on the reconnection rate in two scenarios of magnetic reconnection. The first scenario consists of the "Newton Challenge" problem [Birn , Geophys. Res. Lett. 32, L06105 (2005)]. In this scenario, reconnection is initiated in a plane Harris-type current sheet by temporally limited, spatially varying, inflow of magnetic flux. The second scenario consists of the well-studied island coalescence problem. This scenario starts from an equilibrium containing periodic magnetic islands with parallel current filaments. Due to the attraction between parallel currents, pairs of islands may move toward each other, forming a current sheet in between. This leads to reconnection and ultimately the merging of islands. In either scenario, magnetic reconnection may be considered as being driven by external or internal forcing. Consistent with that interpretation we find that in either case the maximum reconnection rate (electric field) depends approximately linearly on the maximum driving electric field, when other parameters remain unchanged. However, this can be understood mostly from the change of characteristic background parameters; particularly, the increase of the magnetic field strength in the inflow region due to the added magnetic flux. This interpretation is consistent with the result that the maximum of the reconnection electric field is assumed significantly later (tens of Alfven times) than the maximum driving and typically does not match the instantaneous driving electric field. Furthermore, the reconnection rate also depends on the resistivity and the time scale of the driving. (C) 2007 American Institute of Physics. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Birn, J (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 28 TC 14 Z9 14 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD AUG PY 2007 VL 14 IS 8 AR 082306 DI 10.1063/1.2752510 PG 9 WC Physics, Fluids & Plasmas SC Physics GA 206AP UT WOS:000249156600019 ER PT J AU Costes, SV Ponomarev, A Chen, JL Nguyen, D Cucinotta, FA Barcellos-Hoff, MH AF Costes, Sylvain V. Ponomarev, Artem Chen, James L. Nguyen, David Cucinotta, Francis A. Barcellos-Hoff, Mary Helen TI Image-based modeling reveals dynamic redistribution of DNA damage into nuclear sub-domains SO PLOS COMPUTATIONAL BIOLOGY LA English DT Article ID DOUBLE-STRAND BREAKS; PHOSPHORYLATED HISTONE H2AX; HIGH-LET; SIGNALING PATHWAYS; CELLULAR-RESPONSE; SIZE-DISTRIBUTION; MAMMALIAN-CELLS; PARTICLE TRACKS; RADIATION; FOCI AB Several proteins involved in the response to DNA double strand breaks ( DSB) form microscopically visible nuclear domains, or foci, after exposure to ionizing radiation. Radiation- induced foci ( RIF) are believed to be located where DNA damage occurs. To test this assumption, we analyzed the spatial distribution of 53BP1, phosphorylated ATM, and gamma H2AX RIF in cells irradiated with high linear energy transfer ( LET) radiation and low LET. Since energy is randomly deposited along high- LET particle paths, RIF along these paths should also be randomly distributed. The probability to induce DSB can be derived from DNA fragment data measured experimentally by pulsed- field gel electrophoresis. We used this probability in Monte Carlo simulations to predict DSB locations in synthetic nuclei geometrically described by a complete set of human chromosomes, taking into account microscope optics from real experiments. As expected, simulations produced DNA- weighted random ( Poisson) distributions. In contrast, the distributions of RIF obtained as early as 5 min after exposure to high LET ( 1 GeV/ amu Fe) were non- random. This deviation from the expected DNA- weighted random pattern can be further characterized by " relative DNA image measurements.'' This novel imaging approach shows that RIF were located preferentially at the interface between high and low DNA density regions, and were more frequent than predicted in regions with lower DNA density. The same preferential nuclear location was also measured for RIF induced by 1 Gy of low- LET radiation. This deviation from random behavior was evident only 5 min after irradiation for phosphorylated ATM RIF, while gamma H2AX and 53BP1 RIF showed pronounced deviations up to 30 min after exposure. These data suggest that DNA damage - induced foci are restricted to certain regions of the nucleus of human epithelial cells. It is possible that DNA lesions are collected in these nuclear sub- domains for more efficient repair. C1 Lawrence Berkeley Lab, Div Life Sci, Berkeley, CA 94720 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Space Res Assoc, Houston, TX USA. RP Costes, SV (reprint author), Lawrence Berkeley Lab, Div Life Sci, Berkeley, CA 94720 USA. EM svcostes@lbl.gov RI Costes, Sylvain/D-2522-2013 OI Costes, Sylvain/0000-0002-8542-2389 NR 44 TC 61 Z9 62 U1 1 U2 2 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1553-734X EI 1553-7358 J9 PLOS COMPUT BIOL JI PLoS Comput. Biol. PD AUG PY 2007 VL 3 IS 8 BP 1477 EP 1488 AR e155 DI 10.1371/journal.pcbi.0030155 PG 12 WC Biochemical Research Methods; Mathematical & Computational Biology SC Biochemistry & Molecular Biology; Mathematical & Computational Biology GA 214VU UT WOS:000249767100008 PM 17676951 ER PT J AU Bar-Cohen, Y AF Bar-Cohen, Y. TI Electroactive polymers as an enabling materials technology SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE electroactive polymers; artificial muscles; biomimetics; biologically inspired technologies; robotics ID ARTIFICIAL MUSCLES; ACTUATORS; POLYPYRROLE; ELECTRODES AB Natural muscles are the actuators in most of the biological systems that are larger than a bacterium. The drive mechanism of muscles is complex, and they are capable of lifting large loads with short time response in the range of milliseconds. Electroactive polymers (EAPs) are human-made actuators that most closely emulate biological muscles, and therefore they earned the moniker 'artificial muscles'. Initially, EAPs received relatively little attention because of their limited actuation capability. In the last 15 years, a series of EAP materials have emerged that exhibit a significant shape change in response to electrical stimulation. Using these materials as actuators, various novel mechanisms and devices were already demonstrated, including robot fish, catheter steering element, miniature gripper, loudspeaker, active diaphragm, and dust wiper. The impressive advances in improving their actuation strain capability are attracting the attention of engineers and scientists from many different disciplines. These materials are particularly attractive to biornimetic applications, because they can be used to make biologically inspired intelligent robots and other mechanisms. Increasingly, engineers are able to develop EAP-actuated mechanisms that were previously considered science fiction. This article reviews the state-of-the-art challenges and potential applications of EAP materials. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bar-Cohen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yosi@jpl.nasa.gov NR 35 TC 20 Z9 21 U1 4 U2 30 PU PROFESSIONAL ENGINEERING PUBLISHING LTD PI WESTMINISTER PA 1 BIRDCAGE WALK, WESTMINISTER SW1H 9JJ, ENGLAND SN 0954-4100 J9 P I MECH ENG G-J AER JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng. PD AUG PY 2007 VL 221 IS G4 BP 553 EP 564 DI 10.1243/09544100JAERO141 PG 12 WC Engineering, Aerospace; Engineering, Mechanical SC Engineering GA 214NM UT WOS:000249745200009 ER PT J AU Salawitch, RJ AF Salawitch, Ross J. TI Why is there an ozone hole in the atmosphere when there is too much ozone at ground level? SO SCIENTIFIC AMERICAN LA English DT Letter C1 NASA, Jet Prop Lab, Pasadena, CA USA. RP Salawitch, RJ (reprint author), NASA, Jet Prop Lab, Pasadena, CA USA. RI Salawitch, Ross/B-4605-2009 OI Salawitch, Ross/0000-0001-8597-5832 NR 0 TC 0 Z9 0 U1 0 U2 0 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 USA SN 0036-8733 J9 SCI AM JI Sci.Am. PD AUG PY 2007 VL 297 IS 2 BP 102 EP 102 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 189KE UT WOS:000247987000037 ER PT J AU Song, GB Ma, N Lee, HJ Arnold, S AF Song, Gangbing Ma, Ning Lee, Ho-Jun Arnold, Steve TI Design and control of a proof-of-concept variable area exhaust nozzle using shape-memory alloy actuators SO SMART MATERIALS & STRUCTURES LA English DT Article AB There is no reported research in the literature of using shape-memory alloy (SMA) actuators for variable area exhaust nozzles for a jet engine, to the authors' best knowledge. SMA actuators have the advantage of a high power-to-weight ratio and can result in dramatic weight reduction as compared to hydraulic systems. However, the difficulty of using SMA actuators for controlling variable area exhaust nozzles lies in the fact that the temperature near the exhaust nozzle is far higher than the transformation temperature of an SMA actuator. Due to the flexibility and small volume of SMA wire actuators, they can be remotely replaced in a region where the temperature is lower than that of its transformation temperature. By exploiting this fact, this paper presents a novel design of a proof-of-concept variable area exhaust nozzle using shape-memory alloy wire actuators. The SMA actuators are remotely placed away from the exhaust nozzle area so that the environmental temperature is below their transformation temperature. By electrically heating the SMA actuators, the exhaust nozzle will experience an area reduction of up to 40%. Bias springs will apply forces to return the exhaust nozzle to the open-up configuration. A feedback controller based sliding-mode method is used to regulate the SMA actuator position. Experimental results demonstrate that the proposed design meets the desired area variation specifications and shows the promise of a lightweight and simple exhaust nozzle design by using shape-memory alloy actuators. C1 Univ Houston, Dept Mech Engn, Houston, TX 77204 USA. NASA Johnson Space Ctr, Houston, TX 77058 USA. NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Song, GB (reprint author), Univ Houston, Dept Mech Engn, Houston, TX 77204 USA. NR 10 TC 2 Z9 2 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 J9 SMART MATER STRUCT JI Smart Mater. Struct. PD AUG PY 2007 VL 16 IS 4 BP 1342 EP 1347 DI 10.1088/0964-1726/16/4/048 PG 6 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA 199CO UT WOS:000248674000048 ER PT J AU Boynton, WV Sprague, AL Solomon, SC Starr, RD Evans, LG Feldman, WC Trombka, JI Rhodes, EA AF Boynton, William V. Sprague, Ann L. Solomon, Sean C. Starr, Richard D. Evans, Larry G. Feldman, William C. Trombka, Jacob I. Rhodes, Edgar A. TI MESSENGER and the chemistry of Mercury's surface SO SPACE SCIENCE REVIEWS LA English DT Review DE Mercury; MESSENGER; Mercury's surface chemistry; gamma-ray spectrometry; X-ray spectrometry; space missions; planetary surfaces ID IRON-SILICATE FRACTIONATION; REFLECTANCE SPECTRA; HERMEAN REGOLITH; LUNAR PROSPECTOR; ICE DEPOSITS; NEAR-SURFACE; EMISSION-SPECTRA; POLAR ANOMALIES; CALORIS BASIN; RADAR IMAGES AB The instrument suite on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft is well suited to address several of Mercury's outstanding geochemical problems. A combination of data from the Gamma-Ray and Neutron Spectrometer (GRNS) and X-Ray Spectrometer (XRS) instruments will yield the surface abundances of both volatile (K) and refractory (Al, Ca, and Th) elements, which will test the three competing hypotheses for the origin of Mercury's high bulk metal fraction: aerodynamic drag in the early solar nebula, preferential vaporization of silicates, or giant impact. These same elements, with the addition of Mg, Si, and Fe, will put significant constraints on geochemical processes that have formed the crust and produced any later volcanism. The Neutron Spectrometer sensor on the GRNS instrument will yield estimates of the amount of H in surface materials and may ascertain if the permanently shadowed polar craters have a significant excess of H due to water ice. A comparison of the FeO content of olivine and pyroxene determined by the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument with the total Fe determined through both GRNS and XRS will permit an estimate of the amount of Fe present in other forms, including metal and sulfides. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Carnegie Inst Sci, Washington, DC 20015 USA. Catholic Univ Amer, Washington, DC 20064 USA. Comp Sci Corp, Lanham, MD 20706 USA. Inst Plant Sci, Tucson, AZ 85719 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Sprague, AL (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM sprague@lpl.arizona.edu NR 101 TC 23 Z9 23 U1 1 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 AUG PY 2007 VL 131 IS 1-4 BP 85 EP 104 DI 10.1007/s11214-007-9258-3 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238DI UT WOS:000251427100004 ER PT J AU Zuber, MT Aharonson, O Aurnou, JM Cheng, AF Hauck, SA Heimpel, MH Neumann, GA Peale, SJ Phillips, RJ Smith, DE Solomon, SC Stanley, S AF Zuber, Maria T. Aharonson, Oded Aurnou, Jonathan M. Cheng, Andrew F. Hauck, Steven A., II Heimpel, Moritz H. Neumann, Gregory A. Peale, Stanton J. Phillips, Roger J. Smith, David E. Solomon, Sean C. Stanley, Sabine TI The geophysics of Mercury: Current status and anticipated insights from the MESSENGER mission SO SPACE SCIENCE REVIEWS LA English DT Review DE Mercury; MESSENGER; core; rotational state; magnetic dynamos; thermal history ID IRON-SILICATE FRACTIONATION; GENERALIZED CASSINIS LAWS; MAGNETIC-FIELD; MOLTEN CORE; THERMAL EVOLUTION; SPHERICAL-SHELL; PLANET MERCURY; SOLAR-SYSTEM; EARTHS CORE; THERMOELECTRIC DYNAMO AB Current geophysical knowledge of the planet Mercury is based upon observations from ground-based astronomy and flybys of the Mariner 10 spacecraft, along with theoretical and computational studies. Mercury has the highest uncompressed density of the terrestrial planets and by implication has a metallic core with a radius approximately 75% of the planetary radius. Mercury's spin rate is stably locked at 1.5 times the orbital mean motion. Capture into this state is the natural result of tidal evolution if this is the only dissipative process affecting the spin, but the capture probability is enhanced if Mercury's core were molten at the time of capture. The discovery of Mercury's magnetic field by Mariner 10 suggests the possibility that the core is partially molten to the present, a result that is surprising given the planet's size and a surface crater density indicative of early cessation of significant volcanic activity. A present-day liquid outer core within Mercury would require either a core sulfur content of at least several weight percent or an unusual history of heat loss from the planet's core and silicate fraction. A crustal remanent contribution to Mercury's observed magnetic field cannot be ruled out on the basis of current knowledge. Measurements from the MESSENGER orbiter, in combination with continued ground-based observations, hold the promise of setting on a firmer basis our understanding of the structure and evolution of Mercury's interior and the relationship of that evolution to the planet's geological history. C1 MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Case Western Reserve Univ, Dept Geol Sci, Cleveland, OH 44106 USA. Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Zuber, MT (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM Zuber@mit.edu RI Hauck, Steven/A-7865-2008; Neumann, Gregory/I-5591-2013 OI Hauck, Steven/0000-0001-8245-146X; Neumann, Gregory/0000-0003-0644-9944 NR 159 TC 20 Z9 20 U1 0 U2 7 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 AUG PY 2007 VL 131 IS 1-4 BP 105 EP 132 DI 10.1007/s11214-007-9265-4 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238DI UT WOS:000251427100005 ER PT J AU Slavin, JA Krimigis, SM Acuna, MH Anderson, BJ Baker, DN Koehn, PL Korth, H Livi, S Mauk, BH Solomon, SC Zurbuchen, TH AF Slavin, James A. Krimigis, Stamatios M. Acuna, Mario H. Anderson, Brian J. Baker, Daniel N. Koehn, Patrick L. Korth, Haje Livi, Stefano Mauk, Barry H. Solomon, Sean C. Zurbuchen, Thomas H. TI MESSENGER: Exploring mercury's magnetosphere SO SPACE SCIENCE REVIEWS LA English DT Review DE planetary magnetospheres; reconnection; particle acceleration; substorms; Mercury; MESSENGER ID FIELD-ALIGNED CURRENTS; SUBSTORM CURRENT WEDGE; SOLAR-WIND CONTROL; MAGNETIC-FIELD; TERRESTRIAL PLANETS; PLASMA SHEET; THERMOELECTRIC DYNAMO; GEOMAGNETIC-ACTIVITY; DISTANT MAGNETOTAIL; BIRKELAND CURRENTS AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission to Mercury offers our first opportunity to explore this planet's miniature magnetosphere since the brief flybys of Mariner 10. Mercury's magnetosphere is unique in many respects. The magnetosphere of Mercury is among the smallest in the solar system; its magnetic field typically stands off the solar wind only similar to 1000 to 2000 km above the surface. For this reason there are no closed drift paths for energetic particles and, hence, no radiation belts. Magnetic reconnection at the dayside magnetopause may erode the subsolar magnetosphere, allowing solar wind ions to impact directly the regolith. Inductive currents in Mercury's interior may act to modify the solar wind interaction by resisting changes due to solar wind pressure variations. Indeed, observations of these induction effects may be an important source of information on the state of Mercury's interior. In addition, Mercury's magnetosphere is the only one with its defining magnetic flux tubes rooted beneath the solid surface as opposed to an atmosphere with a conductive ionospheric layer. This lack of an ionosphere is probably the underlying reason for the brevity of the very intense, but short-lived, similar to 1-2 min, substorm-like energetic particle events observed by Mariner 10 during its first traversal of Mercury's magnetic tail. Because of Mercury's proximity to the sun, 0.3-0.5 AU, this magnetosphere experiences the most extreme driving forces in the solar system. All of these factors are expected to produce complicated interactions involving the exchange and recycling of neutrals and ions among the solar wind, magnetosphere, and regolith. The electrodynamics of Mercury's magnetosphere are expected to be equally complex, with strong forcing by the solar wind, magnetic reconnection, and pick-up of planetary ions all playing roles in the generation of field-aligned electric currents. However, these field-aligned currents do not close in an ionosphere, but in some other manner. In addition to the insights into magnetospheric physics offered by study of the solar wind-Mercury system, quantitative specification of the "external" magnetic field generated by magnetospheric currents is necessary for accurate determination of the strength and multi-polar decomposition of Mercury's intrinsic magnetic field. MESSENGER's highly capable instrumentation and broad orbital coverage will greatly advance our understanding of both the origin of Mercury's magnetic field and the acceleration of charged particles in small magnetospheres. In this article, we review what is known about Mercury's magnetosphere and describe the MESSENGER science team's strategy for obtaining answers to the outstanding science questions surrounding the interaction of the solar wind with Mercury and its small, but dynamic, magnetosphere. C1 Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. Eastern Michigan Univ, Dept Phys & Astron, Ypsilanti, MI 48197 USA. Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Slavin, JA (reprint author), Goddard Space Flight Ctr, Heliophys Sci Div, Code 670, Greenbelt, MD 20771 USA. EM james.a.slavin@nasa.gov RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Mauk, Barry/E-8420-2017 OI Slavin, James/0000-0002-9206-724X; Mauk, Barry/0000-0001-9789-3797 NR 136 TC 29 Z9 29 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 AUG PY 2007 VL 131 IS 1-4 BP 133 EP 160 DI 10.1007/s11214-007-9154-x PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238DI UT WOS:000251427100006 ER PT J AU Goldsten, JO Rhodes, EA Boynton, WV Feldman, WC Lawrence, DJ Trombka, JI Smith, DM Evans, LG White, J Madden, NW Berg, PC Murphy, GA Gurnee, RS Strohbehn, K Williams, BD Schaefer, ED Monaco, CA Cork, CP Del Eckels, J Miller, WO Burks, MT Hagler, LB DeTeresa, SJ Witte, MC AF Goldsten, John O. Rhodes, Edgar A. Boynton, William V. Feldman, William C. Lawrence, David J. Trombka, Jacob I. Smith, David M. Evans, Larry G. White, Jack Madden, Norman W. Berg, Peter C. Murphy, Graham A. Gurnee, Reid S. Strohbehn, Kim Williams, Bruce D. Schaefer, Edward D. Monaco, Christopher A. Cork, Christopher P. Del Eckels, J. Miller, Wayne O. Burks, Morgan T. Hagler, Lisle B. DeTeresa, Steve J. Witte, Monika C. TI The MESSENGER gamma-ray and neutron spectrometer SO SPACE SCIENCE REVIEWS LA English DT Review DE MESSENGER; Mercury; Gamma-ray spectrometry; X-ray spectrometry; surface composition ID LUNAR PROSPECTOR; MARS ODYSSEY; POLAR ANOMALIES; MERCURY RADAR; ICE DEPOSITS; NORTH-POLE; SURFACE; STABILITY; MOON; SPECTROSCOPY AB A Gamma-Ray and Neutron Spectrometer (GRNS) instrument has been developed as part of the science payload for NASA's Discovery Program mission to the planet Mercury. Mercury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) launched successfully in 2004 and will journey more than six years before entering Mercury orbit to begin a one-year investigation. The GRNS instrument forms part of the geochemistry investigation and will yield maps of the elemental composition of the planet surface. Major elements include H, O, Na, Mg, Si, Ca, Ti, Fe, K, and Th. The Gamma-Ray Spectrometer (GRS) portion detects gamma-ray emissions in the 0.1- to 10-MeV energy range and achieves an energy resolution of 3.5 keV full-width at half-maximum for Co-60 (1332 keV). It is the first interplanetary use of a mechanically cooled Ge detector. Special construction techniques provide the necessary thermal isolation to maintain the sensor's encapsulated detector at cryogenic temperatures (90 K) despite the intense thermal environment. Given the mission constraints, the GRS sensor is necessarily body-mounted to the spacecraft, but the outer housing is equipped with an anticoincidence shield to reduce the background from charged particles. The Neutron Spectrometer (NS) sensor consists of a sandwich of three scintillation detectors working in concert to measure the flux of ejected neutrons in three energy ranges from thermal to similar to 7 MeV. The NS is particularly sensitive to H content and will help resolve the composition of Mercury's polar deposits. This paper provides an overview of the Gamma-Ray and Neutron Spectrometer and describes its science and measurement objectives, the design and operation of the instrument, the ground calibration effort, and a look at some early in-flight data. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. Comp Sci Corp, Sci Programs, Lanham, MD 20706 USA. Sci & Engn Solut Inc, Chagrin Falls, OH 44023 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Goldsten, JO (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM john.goldsten@jhuapl.edu RI Lawrence, David/E-7463-2015 OI Lawrence, David/0000-0002-7696-6667 NR 57 TC 77 Z9 77 U1 0 U2 19 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD AUG PY 2007 VL 131 IS 1-4 BP 339 EP 391 DI 10.1007/s11214-007-9262-7 PG 53 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238DI UT WOS:000251427100011 ER PT J AU Schlemm, CE Starr, RD Ho, GC Bechtold, KE Hamilton, SA Boldt, JD Boynton, WV Bradley, W Fraeman, ME Gold, RE Goldsten, JO Hayes, JR Jaskulek, SE Rossano, E Rumpf, RA Schaefer, ED Strohbehn, K Shelton, RG Thompson, RE Trombka, JI Williams, BD AF Schlemm, Charles E., II Starr, Richard D. Ho, George C. Bechtold, Kathryn E. Hamilton, Sarah A. Boldt, John D. Boynton, William V. Bradley, Walter Fraeman, Martin E. Gold, Robert E. Goldsten, John O. Hayes, John R. Jaskulek, Stephen E. Rossano, Egidio Rumpf, Robert A. Schaefer, Edward D. Strohbehn, Kim Shelton, Richard G. Thompson, Raymond E. Trombka, Jacob I. Williams, Bruce D. TI The x-ray spectrometer on the MESSENGER spacecraft SO SPACE SCIENCE REVIEWS LA English DT Review DE Mercury; MESSENGER; X-ray spectrometry; surface composition; X-ray emissions; elemental composition ID ASTEROID 433 EROS; ELEMENTAL COMPOSITION; MISSION; MERCURY; SURFACE AB NASA's MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) mission will further the understanding of the formation of the planets by examining the least studied of the terrestrial planets, Mercury. During the one-year orbital phase (beginning in 2011) and three earlier flybys (2008 and 2009), the X-Ray Spectrometer (XRS) onboard the MESSENGER spacecraft will measure the surface elemental composition. XRS will measure the characteristic X-ray emissions induced on the surface of Mercury by the incident solar flux. The K alpha lines for the elements Mg, Al, Si, S, Ca, Ti, and Fe will be detected. The 12 degrees field-of-view of the instrument will allow a spatial resolution that ranges from 42 km at periapsis to 3200 km at apoapsis due to the spacecraft's highly elliptical orbit. XRS will provide elemental composition measurements covering the majority of Mercury's surface, as well as potential high-spatial-resolution measurements of features of interest. This paper summarizes XRS's science objectives, technical design, calibration, and mission observation strategy. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 21218 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Univ Arizona, Dept Planetary Sci, Tucson, AZ USA. Goddard Space Flight Ctr, Greenbelt, MD USA. RP Schlemm, CE (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 21218 USA. EM chuck.schlemm@jhuapl.edu RI Ho, George/G-3650-2015 OI Ho, George/0000-0003-1093-2066 NR 16 TC 59 Z9 59 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD AUG PY 2007 VL 131 IS 1-4 BP 393 EP 415 DI 10.1007/s11214-007-9248-5 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238DI UT WOS:000251427100012 ER PT J AU Anderson, BJ Acuna, MH Lohr, DA Scheifele, J Raval, A Korth, H Slavin, JA AF Anderson, Brian J. Acuna, Mario H. Lohr, David A. Scheifele, John Raval, Asseem Korth, Haje Slavin, James A. TI The Magnetometer instrument on MESSENGER SO SPACE SCIENCE REVIEWS LA English DT Review DE Mercury; MESSENGER; Magnetometer; magnetic field; magnetosphere ID MAGNETIC-FIELD EXPERIMENT; CORONAL MASS EJECTIONS; MERCURYS MAGNETOSPHERE; THERMOELECTRIC DYNAMO; CRUSTAL REMANENCE; SPHERICAL-SHELL; MARS; SPACECRAFT; MISSION; DISTURBANCES AB The Magnetometer (MAG) on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission is a low-noise, tri-axial, fluxgate instrument with its sensor mounted on a 3.6-m-long boom. The boom was deployed on March 8, 2005. The primary MAG science objectives are to determine the structure of Mercury's intrinsic magnetic field and infer its origin. Mariner 10 observations indicate a planetary moment in the range 170 to 350 nT R-M(3) (where R-M is Mercury's mean radius). The uncertainties in the dipole moment are associated with the Mariner 10 trajectory and variability of the measured field. By orbiting Mercury, MESSENGER will significantly improve the determination of dipole and higher-order moments. The latter are essential to understanding the thermal history of the planet. MAG has a coarse range, +/- 51,300 nT full scale (1.6-nT resolution), for pre-flight testing, and a fine range, +/- 1,530 nT full scale (0.047-nT resolution), for Mercury operation. A magnetic cleanliness program was followed to minimize variable and static spacecraft-generated fields at the sensor. Observations during and after boom deployment indicate that the fixed residual field is less than a few nT at the location of the sensor, and initial observations indicate that the variable field is below 0.05 nT at least above about 3 Hz. Analog signals from the three axes are low-pass filtered (10-Hz cutoff) and sampled simultaneously by three 20-bit analog-to-digital converters every 50 ms. To accommodate variable telemetry rates, MAG provides 11 output rates from 0.01 s(-1) to 20 s(-1). Continuous measurement of fluctuations is provided with a digital 1-10 Hz bandpass filter. This fluctuation level is used to trigger high-time-resolution sampling in eight-minute segments to record events of interest when continuous high-rate sampling is not possible. The MAG instrument will provide accurate characterization of the intrinsic planetary field, magnetospheric structure, and dynamics of Mercury's solar wind interaction. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Anderson, BJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM brian.anderson@jhuapl.edu RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X NR 70 TC 125 Z9 125 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 AUG PY 2007 VL 131 IS 1-4 BP 417 EP 450 DI 10.1007/s11214-007-9246-7 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238DI UT WOS:000251427100013 ER PT J AU Cavanaugh, JF Smith, JC Sun, XL Bartels, AE Ramos-Izquierdo, L Krebs, DJ McGarry, JF Trunzo, R Novo-Gradac, AM Britt, JL Karsh, J Katz, RB Lukemire, AT Szymkiewicz, R Berry, DL Swinski, JP Neumann, GA Zuber, MT Smith, DE AF Cavanaugh, John F. Smith, James C. Sun, Xiaoli Bartels, Arlin E. Ramos-Izquierdo, Luis Krebs, Danny J. McGarry, Jan F. Trunzo, Raymond Novo-Gradac, Anne Marie Britt, Jamie L. Karsh, Jerry Katz, Richard B. Lukemire, Alan T. Szymkiewicz, Richard Berry, Daniel L. Swinski, Joseph P. Neumann, Gregory A. Zuber, Maria T. Smith, David E. TI The Mercury Laser Altimeter instrument for the MESSENGER mission SO SPACE SCIENCE REVIEWS LA English DT Review DE Mercury; MESSENGER; topography; laser altimeter ID MARS AB The Mercury Laser Altimeter (MLA) is one of the payload science instruments on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission, which launched on August 3, 2004. The altimeter will measure the round-trip time of flight of transmitted laser pulses reflected from the surface of the planet that, in combination with the spacecraft orbit position and pointing data, gives a high-precision measurement of surface topography referenced to Mercury's center of mass. MLA will sample the planet's surface to within a 1-m range error when the line-of-sight range to Mercury is less than 1,200 km under spacecraft nadir pointing or the slant range is less than 800 km. The altimeter measurements will be used to determine the planet's forced physical librations by tracking the motion of large-scale topographic features as a function of time. MLA's laser pulse energy monitor and the echo pulse energy estimate will provide an active measurement of the surface reflectivity at 1,064 nm. This paper describes the instrument design, prelaunch testing, calibration, and results of postlaunch testing. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Swales Aerosp, Beltsville, MD 20705 USA. Orbital Sci, Greenbelt, MD 20770 USA. Space Power Elect, Kathleen, GA 31047 USA. MIT, Cambridge, MA 02129 USA. RP Cavanaugh, JF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM john.f.cavanaugh@nasa.gov RI Sun, Xiaoli/B-5120-2013; McGarry, Jan/C-4109-2013; Neumann, Gregory/I-5591-2013 OI Neumann, Gregory/0000-0003-0644-9944 NR 14 TC 72 Z9 73 U1 4 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD AUG PY 2007 VL 131 IS 1-4 BP 451 EP 479 DI 10.1007/s11214-007-9273-4 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238DI UT WOS:000251427100014 ER PT J AU Srinivasan, DK Perry, ME Fielhauer, KB Smith, DE Zuber, MT AF Srinivasan, Dipak K. Perry, Mark E. Fielhauer, Karl B. Smith, David E. Zuber, Maria T. TI The radio frequency subsystem and radio science on the MESSENGER mission SO SPACE SCIENCE REVIEWS LA English DT Review DE MESSENGER; Mercury; telecommunications system; radio science; gravity science; spacecraft tracking; gravitational field ID OCCULTATION MEASUREMENTS; MERCURY; MARS; CORE; ATMOSPHERE; TOPOGRAPHY; SHAPE AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) Radio Frequency (RF) Telecommunications Subsystem is used to send commands to the spacecraft, transmit information on the state of the spacecraft and science-related observations, and assist in navigating the spacecraft to and in orbit about Mercury by providing precise observations of the spacecraft's Doppler velocity and range in the line of sight to Earth. The RF signal is transmitted and received at X-band frequencies (7.2 GHz uplink, 8.4 GHz downlink) by the NASA Deep Space Network. The tracking data from MESSENGER will contribute significantly to achieving the mission's geophysics objectives. The RF subsystem, as the radio science instrument, will help determine Mercury's gravitational field and, in conjunction with the Mercury Laser Altimeter instrument, help determine the topography of the planet. Further analysis of the data will improve the knowledge of the planet's orbital ephemeris and rotation state. The rotational state determination includes refined measurements of the obliquity and forced physical libration, which are necessary to characterize Mercury's core state. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Srinivasan, DK (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM dipak.srinivasan@jhuapl.edu RI Perry, Mark/B-8870-2016 OI Perry, Mark/0000-0003-1600-6856 NR 24 TC 16 Z9 16 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD AUG PY 2007 VL 131 IS 1-4 BP 557 EP 571 DI 10.1007/s11214-007-9270-7 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238DI UT WOS:000251427100017 ER PT J AU Masson, PJ Brown, GV Soban, DS Luongo, CA AF Masson, P. J. Brown, G. V. Soban, D. S. Luongo, C. A. TI HTS machines as enabling technology for all-electric airborne vehicles SO SUPERCONDUCTOR SCIENCE & TECHNOLOGY LA English DT Article ID AIRCRAFT PROPULSION; DESIGN AB Environmental protection has now become paramount as evidence mounts to support the thesis of human activity-driven global warming. A global reduction of the emissions of pollutants into the atmosphere is therefore needed and new technologies have to be considered. A large part of the emissions come from transportation vehicles, including cars, trucks and airplanes, due to the nature of their combustion-based propulsion systems. Our team has been working for several years on the development of high power density superconducting motors for aircraft propulsion and fuel cell based power systems for aircraft. This paper investigates the feasibility of all-electric aircraft based on currently available technology. Electric propulsion would require the development of high power density electric propulsion motors, generators, power management and distribution systems. The requirements in terms of weight and volume of these components cannot be achieved with conventional technologies; however, the use of superconductors associated with hydrogen-based power plants makes possible the design of a reasonably light power system and would therefore enable the development of all-electric aero-vehicles. A system sizing has been performed both for actuators and for primary propulsion. Many advantages would come from electrical propulsion such as better controllability of the propulsion, higher efficiency, higher availability and less maintenance needs. Superconducting machines may very well be the enabling technology for all-electric aircraft development. C1 FAMU FSU Coll Engn, Tallahassee, FL 32310 USA. Ctr Adv Power Syst, Tallahassee, FL 32310 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. Georgia Tech, Aerosp Syst Design Lab, Atlanta, GA USA. RP Masson, PJ (reprint author), FAMU FSU Coll Engn, Tallahassee, FL 32310 USA. EM masson@caps.fsu.edu; Gerald.V.Brown@grc.nasa.gov; danielle.soban@ae.gatech.edu; luongo@magnet.fsu.edu RI Masson, Philippe/G-6408-2012 NR 12 TC 31 Z9 31 U1 4 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-2048 J9 SUPERCOND SCI TECH JI Supercond. Sci. Technol. PD AUG PY 2007 VL 20 IS 8 BP 748 EP 756 DI 10.1088/0953-2048/20/8/005 PG 9 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 198XO UT WOS:000248661000008 ER PT J AU Mosca, HO Bozzolo, G AF Mosca, Hugo O. Bozzolo, Guillermo TI Surface energies of the solid solutions between Ti, V, Cr, Zr, Nb, Mo, Hf, Ta, and W SO SURFACE SCIENCE LA English DT Article DE surface energy; computer simulations; Monte Carlo simulations ID EMBEDDED-ATOM METHOD; HIGH-INDEX SURFACES; ANISOTROPY ANALYSIS; THIN-FILMS; METALS; CRYSTAL; ALLOYS; TEMPERATURE; STRESS; COPPER AB The surface energy for different surface orientations of the solid solutions as a function of concentration formed by Ti, V, Cr, Zr, Nb, Mo, Hf, Ta, and W is computed and analyzed using the BFS method for alloys. Similarities and differences among the different binary alloys are examined in terms of strain and chemical effects. (c) 2007 Elsevier B.V. All rights reserved. C1 Ohio Aerosp Inst, Cleveland, OH 44142 USA. Comis Nacl Energia Atom, UA Fis, San Martin, Pcia De Bs As, Argentina. NASA, Glen Res Ctr, Cleveland, OH 44135 USA. RP Bozzolo, G (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. EM GuillermoBozzolo@oai.org NR 36 TC 7 Z9 7 U1 1 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0039-6028 J9 SURF SCI JI Surf. Sci. PD AUG 1 PY 2007 VL 601 IS 15 BP 3224 EP 3232 DI 10.1016/j.susc.2007.05.038 PG 9 WC Chemistry, Physical; Physics, Condensed Matter SC Chemistry; Physics GA 202DJ UT WOS:000248881900011 ER PT J AU Hall, TM Jewson, S AF Hall, Timothy M. Jewson, Stephen TI Statistical modelling of North Atlantic tropical cyclone tracks SO TELLUS SERIES A-DYNAMIC METEOROLOGY AND OCEANOGRAPHY LA English DT Article; Proceedings Paper CT Workshop of the International-Research-Institute-for-Climate-and-Society CY MAR, 2006 CL Columbia Univ, Palisades, NY SP US Natl Sci Fdn, Columbia Univ, ADVANCE Programm, IRI, Columbia Univ, NSF IGERT Joint Program Appl Math & Environm Sci, NSF HO Columbia Univ ID HURRICANE RISK; SIMULATION AB We present a statistical model of North Atlantic tropical cyclone tracks from genesis site through lysis. To propagate tracks we use the means and variances of latitudinal and longitudinal displacements and model the remaining anomalies as autoregressive. Coefficients are determined by averaging near-neighbour historical track data, with 'near' determined optimally by using jackknife out-of-sample validation to maximize the likelihood of the observations. The number of cyclones in a simulated year is sampled randomly from the historical record, and the cyclone genesis sites are simulated with a spatial probability density function using kernels with optimized bandwidths. Simulated cyclones suffer lysis with a probability again determined from optimal averaging of historical lysis rates. We evaluate the track model by comparing an ensemble of 1950-2003 simulations to the historical record using several diagnostics, including landfall rates. In most regions, but not all, the observations fall within the variability across the ensemble members, indicating that the simulations and observations are statistically indistinguishable. An intensity component to the TC model, necessary for risk assessment applications, is currently under development. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Risk Management Solut, London, England. RP Hall, TM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM thall@giss.nasa.gov NR 13 TC 46 Z9 48 U1 0 U2 7 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0280-6495 J9 TELLUS A JI Tellus Ser. A-Dyn. Meteorol. Oceanol. PD AUG PY 2007 VL 59 IS 4 BP 486 EP 498 DI 10.1111/j.1600-0870.2007.00240.x PG 13 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA 197GS UT WOS:000248543200009 ER PT J AU Zerefos, CS Eleftheratos, K Zanis, P Balis, DS Tselioudis, G AF Zerefos, Christos S. Eleftheratos, Kostas Zanis, Prodromos Balis, Dimitris S. Tselioudis, George TI Search for man-made cirrus contrails over Southeast Asia SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES LA English DT Article; Proceedings Paper CT 6th EACE Meeting on Climate-Chemistry Interaction - Importance of Atmospheric Circulation and Water Vapor CY SEP 19-21, 2005 CL Shanghai, PEOPLES R CHINA ID PART I; CLOUDS; ISCCP; AVIATION; CLIMATE; IMPACT AB In this study we examine the effect of natural perturbations on cirrus cloud cover in the tropics and we look for possible signal of cirrus contrails in tropical air traffic regions focussing on Southeast Asia, a region that has received much less attention than the well investigated North Atlantic and North American air traffic corridors. The analysis is based on the latest version of the ISCCP D2 cirrus cloud dataset and covers the period 1984 2000. Four parameters were examined for their relation with cirrus cloud trends: deep convective clouds from ISCCP, vertical velocities, relative humidity and air temperature at 200 mb from ECMWF/ERA40. The results show that there is a strong correlation between cirrus clouds and dynamical parameters (deep convective clouds, vertical velocities) over Southeast Asia, explaining a significant part of the tropical cirrus cloud variability. After removing seasonality, the ENSO signal becomes dominant on cirrus, on deep convective clouds and on vertical velocities over regions of the western and the eastern tropical Pacific Ocean. Over Southeast Asia, the average decrease in cirrus during the strong 1997/98 El Nino event was about 6 % cloud cover or similar to 25 % of the regional mean. In order to search for possible signal of cirrus contrails over S. E. Asia, we calculated trends in cirrus coverage over tropical regions with high air traffic after removing the ENSO effect. The results show that there is a small positive trend in cirrus clouds over the S. E. Asia air corridors during winter (+0.1 % cover/decade), which is not statistically significant and is related to small positive trends in deep convective clouds. In summer, cirrus clouds are anti-correlated with deep convective clouds over this region and the trends are opposite. The negative trends in cirrus clouds, which are observed in the summer (4.5 % cover/ decade), are related to trends in dynamical and thermo- dynamical parameters. It is shown that cirrus clouds are statistically significant correlated with vertical velocities and air temperature at 200 mb (correlations of -0.7 and -0.6, respectively), explaining the highest part of the long-term variability of cirrus clouds over S. E. Asia. Over the Caribbean air corridors, on the other hand, there are significant increases in cirrus cloudiness by about 2.5% per decade in winter (99% confidence level) and 2.7% cover/ decade in the summer (95% confidence level), part of which is also related to trends in dynamical and thermo-dynamical parameters. According to our findings, it is difficult to detect possible effects of regional persistent contrails on cirrus cloud trends over the S. E. Asia air traffic corridors. This is because in winter there are not statistically significant trends in cirrus clouds and in summer trends in dynamics and thermo-dynamics mask this issue. Taking also into account that flight frequencies and fuel consumption are moderate over the tropical air traffic corridors, it makes it even more difficult to detect and quantify any possible anthropogenic effects. C1 Univ Athens, Lab Climatol & Atmospher Environm, Athens, Greece. Acad Athens, Fdn Biomed Res, Athens, Greece. Natl Observ Athens, Athens, Greece. Acad Athens, Res Ctr Atmospher Phys & Climatol, Athens, Greece. Univ Thessaloniki, Lab Atmospher Phys, Thessaloniki, Greece. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Zerefos, CS (reprint author), Univ Athens, Lab Climatol & Atmospher Environm, Athens, Greece. EM zerefos@geol.uoa.gr RI Zanis, Prodromos/B-5598-2015; OI Balis, Dimitris/0000-0003-1161-7746 NR 15 TC 5 Z9 5 U1 0 U2 4 PU CHINESE GEOSCIENCE UNION PI TAIPEI PA PO BOX 23-59, TAIPEI 10764, TAIWAN SN 1017-0839 J9 TERR ATMOS OCEAN SCI JI Terr. Atmos. Ocean. Sci. PD AUG PY 2007 VL 18 IS 3 BP 459 EP 474 DI 10.3319/TAO.2007.18.3.459 PG 16 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Oceanography SC Geology; Meteorology & Atmospheric Sciences; Oceanography GA 222PR UT WOS:000250309900004 ER PT J AU Juang, HMH Tao, WK Zeng, X Shie, CL Lang, S Simpson, J AF Juang, Hann-Ming Henry Tao, Wei-Kuo Zeng, Xiping Shie, Chung-Lin Lang, Stephen Simpson, Joanne TI Parallelization of the NASA Goddard cumulus ensemble model for massively parallel computing SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES LA English DT Article DE domain decomposition; message passing interface; massively parallel; computing; cloud-resolving model; numerical weather prediction ID GENERATED MOIST CONVECTION; TIME-INTEGRATION SCHEMES; AREA ATMOSPHERIC MODELS; BULK ICE SCHEME; PART I; PREDICTION MODEL; CLOUD SYSTEMS; SQUALL LINES; TOGA COARE; SIMULATIONS AB Massively parallel computing, using a message passing interface (MPI), has been implemented into a three-dimensional version of the Goddard Cumulus Ensemble (GCE) model. The implementation uses the domainresemble concept to design a code structure for both the whole domain and sub-domains after decomposition. Instead of inserting a group of MPI related statements into the model routine, these statements are packed into a single routine. In other words, only a single call statement to the model code is utilized once in a place, thus there is minimal impact on the original code. Therefore, the model is easily modified and/or managed by the model developers and/or users, who have little knowledge of massively parallel computing. The model decomposition is highly flexible such that the entire model domain can be sliced into any number of partial domains in one- or twodimensional decomposition. Data exchange is through a halo-region, which is overlaid with neighboring partial domains. A halo-region is also known as a ghost-cell region. For reproducibility purposes, transposing data among tasks into different decompositions is required, such as Fourier transform and full domain summation. The well-behaved performance of the implemented codes with anelastic and compressible versions on three different computing platforms indicates a successful implementation.. The parallelization of both versions has speedup of 99% for up to 256 tasks. The anelastic version has better speedup and efficiency because its numerical algorithm is preferred by the parallelization than that of the compressible version. C1 NOAA, Environm Model Ctr, NCEP, Washington, DC 20230 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD USA. Univ Maryland Baltimore Cty, Goddard Space Sci & Technol Ctr, Baltimore, MD USA. Sci Syst & Appl Inc, Lanham, MD USA. RP Juang, HMH (reprint author), NOAA, Environm Model Ctr, NCEP, Washington, DC 20230 USA. EM Henry.Juang@noaa.gov NR 43 TC 7 Z9 7 U1 0 U2 3 PU CHINESE GEOSCIENCE UNION PI TAIPEI PA PO BOX 23-59, TAIPEI 10764, TAIWAN SN 1017-0839 J9 TERR ATMOS OCEAN SCI JI Terr. Atmos. Ocean. Sci. PD AUG PY 2007 VL 18 IS 3 BP 593 EP 622 DI 10.3319/TAO.2007.18.3.593 PG 30 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Oceanography SC Geology; Meteorology & Atmospheric Sciences; Oceanography GA 222PR UT WOS:000250309900011 ER PT J AU Chambers, JQ Asner, GP Morton, DC Anderson, LO Saatch, SS Espirito-Santo, FDB Palace, M Souza, C AF Chambers, Jeffrey Q. Asner, Gregory P. Morton, Douglas C. Anderson, Liana O. Saatch, Sassan S. Espirito-Santo, Fernando D. B. Palace, Michael Souza, Carlos, Jr. TI Regional ecosystem structure and function: ecological insights from remote sensing of tropical forests SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID RESOLUTION SATELLITE DATA; SPACEBORNE IMAGING SPECTROSCOPY; BIOSPHERE-ATMOSPHERE EXPERIMENT; BRAZILIAN AMAZON; RAIN-FOREST; ABOVEGROUND BIOMASS; CARBON EMISSIONS; FOOTPRINT LIDAR; GLOBAL CHANGE; TERRA MODIS AB Ecological studies in tropical forests have long been plagued by difficulties associated with sampling the crowns of large canopy trees and large inaccessible regions, such as the Amazon basin. Recent advances in remote sensing have overcome some of these obstacles, enabling progress towards tackling difficult ecological problems. Breakthroughs have helped transform the dialog between ecology and remote sensing, generating new regional perspectives on key environmental gradients and species assemblages with ecologically relevant measures such as canopy nutrient and moisture content, crown area, leaf-level drought responses, woody tissue and surface litter abundance, phenological patterns, and land-cover transitions. Issues that we address here include forest response to altered precipitation regimes, regional disturbance and land-use patterns, invasive species and landscape carbon balance. C1 Tulane Univ, New Orleans, LA 70118 USA. Carnegie Inst, Dept Global Ecol, Stanford, CA 94305 USA. Univ Maryland, Dept Geog, College Pk, MD 20742 USA. Univ Oxford, Ctr Environm, Environm Change Inst, Oxford OX1 3QY, England. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. Inst Homem & Meio Ambiente Amazonia Imazon, Belem, Para, Brazil. RP Chambers, JQ (reprint author), Tulane Univ, 310 Dinwiddie Hall, New Orleans, LA 70118 USA. EM chambers@tulane.edu RI Morton, Douglas/D-5044-2012; Anderson, Liana/G-8389-2012; Chambers, Jeffrey/J-9021-2014; Asner, Gregory/G-9268-2013; Espirito-Santo, Fernando/O-4371-2014 OI Anderson, Liana/0000-0001-9545-5136; Chambers, Jeffrey/0000-0003-3983-7847; Asner, Gregory/0000-0001-7893-6421; Espirito-Santo, Fernando/0000-0001-7497-3639 NR 90 TC 124 Z9 130 U1 6 U2 75 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD AUG PY 2007 VL 22 IS 8 BP 414 EP 423 DI 10.1016/j.tree.2007.05.001 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 198OT UT WOS:000248638100006 PM 17493704 ER PT J AU Gamayunov, KV Khazanov, GV AF Gamayunov, K. V. Khazanov, G. V. TI Effect of oblique electromagnetic ion cyclotron waves on relativistic electron scattering: Combined Release and Radiation Effects Satellite (CRRES)-based calculation SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PITCH-ANGLE; DIFFUSION-COEFFICIENTS; GEOMAGNETIC STORMS; MAGNETIC STORM; EMIC WAVES; PRECIPITATION; ACCELERATION; ENERGIES; BELT AB [1] We consider the effect of oblique electromagnetic ion cyclotron (EMIC) waveson relativistic electron scattering in the outer radiation belt (RB) using simultaneous observations of plasma and wave parameters from Combined Release and Radiation Effects Satellite (CRRES). The main findings can be summarized as follows. First, in comparison with field-aligned waves, intermediate and highly oblique distributions decrease the range of pitch angles subject to diffusion and reduce the local scattering rate by about an order of magnitude at pitch angles where the principle vertical bar n vertical bar = 1 resonances operate. Oblique waves allow the vertical bar n vertical bar > 1 resonances to operate, extending the range of local pitch angle diffusion down to the loss cone, and increasing the diffusion at lower pitch angles by orders of magnitude. Second, the local diffusion coefficients derived from CRRES data are qualitatively similar to the local results obtained for prescribed plasma/wave parameters. Consequently, it is likely that the bounce-averaged diffusion coefficients, if estimated from concurrent data, will exhibit the dependencies similar to those we found for model calculations. Third, in comparison with field-aligned waves, intermediate and highly oblique waves decrease the bounce-averaged scattering rate near the edge of the equatorial loss cone by orders of magnitude if the electron energy does not exceed a threshold ( similar to 2-5 MeV) depending on specified plasma and/or wave parameters. Lastly, for greater electron energies, oblique waves operating the vertical bar n vertical bar > 1 resonances are more effective and provide the same bounce-averaged diffusion rate near the loss cone as field-aligned waves do. C1 NASA, Natl Space Sci & Technol Ctr, Marshall Space Flight Ctr VP62, Dept Space Sci, Huntsville, AL 35805 USA. RP Gamayunov, KV (reprint author), NASA, Natl Space Sci & Technol Ctr, Marshall Space Flight Ctr VP62, Dept Space Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM konstantin.gamayunov@msfc.nasa.gov; george.khazanov@msfc.nasa.gov RI Gamayunov, Konstantin/A-8505-2009 OI Gamayunov, Konstantin/0000-0002-8768-8527 NR 24 TC 5 Z9 5 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 JUL 31 PY 2007 VL 112 IS A7 AR A07220 DI 10.1029/2007JA012300 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 198DB UT WOS:000248606100002 ER PT J AU Suh, JO Tu, KN Tamura, N AF Suh, J. O. Tu, K. N. Tamura, N. TI Dramatic morphological change of scallop-type Cu6Sn5 formed on (001) single crystal copper in reaction between molten SnPb solder and Cu SO APPLIED PHYSICS LETTERS LA English DT Article ID TIN; JOINTS AB Wetting reaction between molten Sn-based solders and Cu produces scallop-type Cu6Sn5. In the present wetting study, a (001) single crystal Cu is used as substrate and a dramatic change in the morphology of Cu6Sn5 is observed: instead of scallop type, the authors observed a rooftop-type Cu6Sn5 grains, elongated along two preferred orientation directions. This was confirmed by electron beam backscattered diffraction and white beam synchrotron x-ray microdiffraction. The results indicate that the nucleation, growth, and ripening behavior of Cu6Sn5 on single crystal substrate can be quite different from the conventional case of wetting on randomly oriented polycrystalline Cu substrates. (c) 2007 American Institute of Physics. C1 Univ Calif Los Angeles, Dept Mat Sci & Engn, Los Angeles, CA 90095 USA. Ernest Orlando Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Suh, JO (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 13 TC 51 Z9 52 U1 3 U2 25 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 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUL 30 PY 2007 VL 91 IS 5 AR 051907 DI 10.1063/1.2761840 PG 3 WC Physics, Applied SC Physics GA 197ZJ UT WOS:000248595800035 ER PT J AU Bonifacie, M Jendrzejewski, N Agrinier, P Coleman, M Pineau, F Javoy, M AF Bonifacie, Magali Jendrzejewski, Nathalie Agrinier, Pierre Coleman, Max Pineau, Francoise Javoy, Marc TI Pyrohydrolysis-IRMS determination of silicate chlorine stable isotope compositions. Application to oceanic crust and meteorite samples SO CHEMICAL GEOLOGY LA English DT Article DE delta Cl-37; reference rock; chlorine geochernical cycle; MORB; serpentinite ID ION MASS-SPECTROMETRY; GEODYNAMIC CYCLE; DELTA-CL-37; CL; RATIOS; FLUIDS; RIDGE; DECOMPOSITION; FLUORINE; HALOGENS AB This contribution describes the optimization of chlorine extraction from silicate samples by pyrohydrolysis prior to the precise determination of Cl stable-isotope compositions (637 Cl) by gas source, dual inlet Isotope Ratio Mass Spectrometry (IRMS) on CH(3)Clg. The complete method was checked on three international reference materials for Cl-content and two laboratory glass standards. Whole procedure blanks are lower than 0. 5 mu mol, corresponding to less than 10 wt.% of most of the sample chloride analysed. In the absence of international chlorine isotope rock, we report here Cl extracted compared to accepted Cl contents and reproducibilities on Cl and delta Cl-37 measurements for the standard rocks. After extraction, the Cl contents of the three international references compared within error with the accepted values (mean yield = 94 +/-10%) with reproducibilities better than 12% (10). The laboratory glass standards - andesite SO100DS92 and phonolite S9(2) - were used specifically to test the effect of chloride amount on the measurements. They gave Cl extraction yields of 100 +/-6% (1 sigma-; n = 15) and 105 +/- 8% (1 sigma-; n = 7), respectively, with delta Cl-37 values of -0.51 0.14%o and -0.39 0.17%o (1g). In summary, for silicate samples with Cl contents between 39 and 9042 ppm, the Pyrohydrolysis/HPLC method leads to overall CI extraction yields of 100 8%, reproducibilities on Cl contents of 7% and on delta Cl-37 measurements of 0.12%o (all 1 sigma). The method was further applied to ten silicate rocks of various mineralogy and chemistry (meteorite, fresh MORB glasses, altered basalts and setpentinized peridotites) chosen for their large range of Cl contents (70-2156 ppm) and their geological significance. delta Cl-37 values range between -2.33 and -0.50%o. These strictly negative values contrast with the large range and mainly positive values previously reported for comparable silicate samples and shown here to be affected by analytical problems. Thus we propose a preliminary, revised terrestrial CI cycle, mainly dominated by negative and zero delta Cl-37 values. (C) 2007 Elsevier B.V. All rights reserved. C1 Univ Paris 07, Inst Phys Globe Paris, CNRS, UMR 7154,Lab Geochim Isotopes Stables, F-75251 Paris 05, France. CALTECH, Jet Prop Lab, Ctr Life Detect, Pasadena, CA 91109 USA. Univ Reading, Postgrad Res Inst Sedimentol, Reading RG6 6AB, Berks, England. RP Bonifacie, M (reprint author), CALTECH, Div Geol & Planetary Sci, 1200 Calif Blvd,MC 100-23, Pasadena, CA 91125 USA. EM bonifaci@gps.caltech.edu RI Bonifacie, Magali/A-5656-2011; Coleman, Max/A-1303-2007 OI Coleman, Max/0000-0002-5514-1826 NR 45 TC 40 Z9 40 U1 3 U2 23 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 J9 CHEM GEOL JI Chem. Geol. PD JUL 30 PY 2007 VL 242 IS 1-2 BP 187 EP 201 DI 10.1016/j.chemgeo.2007.03.012 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 195SZ UT WOS:000248433400011 ER PT J AU Weishampel, JF Drake, JB Cooper, A Blair, JB Hofton, M AF Weishampel, John F. Drake, Jason B. Cooper, Amanda Blair, J. Bryan Hofton, Michelle TI Forest canopy recovery from the 1938 hurricane and subsequent salvage damage measured with airborne LiDAR SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE disturbance; ecosystem recovery; forest canopy; Harvard Forest; hurricane; land use; legacy; LiDAR; LISA; spatial autocorrelation; vertical structure ID CENTRAL NEW-ENGLAND; DOUGLAS-FIR FORESTS; LAND-USE HISTORY; WAVE-FORM LIDAR; SPATIAL ASSOCIATION; CATASTROPHIC WIND; LASER ALTIMETER; HEIGHT PROFILES; HARDWOOD FOREST; NEW-HAMPSHIRE AB The structure of a forest canopy often reflects its disturbance history. Such signatures of past disturbances or legacies can influence bow the ecosystem functions across broad spatio-temporal scales. The 1938 hurricane and ensuing salvage operations which swept through New England represent the most recent large, infrequent disturbance (LID) in this region. Though devastating (downing similar to 70% of the timber at Harvard Forest), the disturbance was not indiscriminate-, it left behind a heterogeneous landscape comprised of different levels of canopy damage. We analyzed large-footprint LiDAR, from the Prospect Hill tract at Harvard Forest in central Massachusetts, to assess whether damage to the forest structure from the hurricane and subsequent timber extraction could be discerned after - 65 years. Differences in LiDAR-derived measures of canopy height and vertical diversity were a function of the degree of damage from the 1938 hurricane and the predominant tree species which is, in part, a function of land use history. Higher levels of damage corresponded to slightly shorter canopies with a less even vertical distribution of return from the ground to the top. In addition, differences in canopy topography as revealed by spatial autocorrelation of canopy top heights were found among the damage classes. Less disturbed stands were characterized by lower levels of local autocorrelation for canopy height and higher levels of vertical diversity of LiDAR returns. These differences in canopy structure reveal that the forest tract has not completely recovered from the 1938 LID and salvage regime, which may have implications on arboreal and understory habitat and other ecosystem functions. (c) 2007 Elsevier Inc. All rights reserved. C1 Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. Univ Maryland, Dept Geog, College Pk, MD 20742 USA. USDA, Forest Serv, Tallahassee, FL USA. RP Weishampel, JF (reprint author), Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. EM jweisham@mail.ucf.edu RI Khachadourian, Diana/C-8513-2012; Blair, James/D-3881-2013; Beckley, Matthew/D-4547-2013 NR 71 TC 22 Z9 24 U1 5 U2 19 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 JUL 30 PY 2007 VL 109 IS 2 BP 142 EP 153 DI 10.1016/j.rse.2006.12.016 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 183LE UT WOS:000247573500002 ER PT J AU Beckley, BD Lemoine, FG Luthcke, SB Ray, RD Zelensky, NP AF Beckley, B. D. Lemoine, F. G. Luthcke, S. B. Ray, R. D. Zelensky, N. P. TI A reassessment of global and regional mean sea level trends from TOPEX and Jason-1 altimetry based on revised reference frame and orbits SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TERRESTRIAL REFERENCE FRAME; STATE BIAS; SERVICE; MODEL; WIND; RISE AB Mean sea level trends from TOPEX and Jason-1 altimeter data are recomputed using unified geophysical modeling and the new ITRF2005 terrestrial reference frame for the entire altimetric time series, with consistent orbits based on satellite laser ranging (SLR) and DORIS tracking data. We obtain a global rate of 3.36 +/- 0.41 mm/yr over the 14 year period from 1993 to 2007. The regional sea level trends computed with the new reference frame show significant north/south hemispherical offsets of +/- 1.5 mm/yr relative to trends based on the previous 1995-era frame. Regional sea level trend comparisons for the time periods of 1993-1999 and 1999-2005 reveal strong basin-scale polarities and pronounced inter-decadal variability, with a relative increase in the global mean sea level trend of 1.5 +/- 0.7 mm/yr in the latter seven years. C1 Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Beckley, BD (reprint author), Stinger Ghaffarian Technol Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. EM brian.d.beckley@gsfc.nasa.gov RI Ray, Richard/D-1034-2012; Luthcke, Scott/D-6283-2012; Lemoine, Frank/D-1215-2013 NR 37 TC 98 Z9 101 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2007 VL 34 IS 14 AR L14608 DI 10.1029/2007GL030002 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 195OC UT WOS:000248420500006 ER PT J AU Fu, Q Hu, YX Yang, Q AF Fu, Qiang Hu, Yongxiang Yang, Qiong TI Identifying the top of the tropical tropopause layer from vertical mass flux analysis and CALIPSO lidar cloud observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CIRRUS CLOUDS; RADIATIVE PROPERTIES; ACCURATE PARAMETERIZATION; LOWER STRATOSPHERE; CLIMATE MODELS; TRANSPORT; CIRCULATION; TROPOSPHERE; OZONESONDES; BALANCE AB We identify the top of the tropical tropopause layer (TTL) by analyzing the vertical mass flux profile based on radiative transfer calculations employing observed atmospheric profiles and cloud information. We find that the top of the TTL is located at similar to 18.7 km ( 70 mb). We have analyzed the CALIPSO lidar cloud observations from June 2006 to February 2007, which indicates that almost no clouds occur above 19 km, consistent with the top of TTL based on vertical mass flux analyses. The total cloud fractions between 20 degrees S and 20 degrees N are about 0.05% at 18.5 km, 0.5% at 18.0 km and 5% at 17.0 km, where the clouds with optical depth larger than 0.5 contribute up to one tenth of these total cloud fractions. The clouds above 17 km mainly originate over the West Pacific, South America, Central Africa, and South Asia. C1 Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Fu, Q (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA. EM qfu@atmos.washington.edu RI Hu, Yongxiang/K-4426-2012 NR 26 TC 44 Z9 46 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2007 VL 34 IS 14 AR L14813 DI 10.1029/2007GL030099 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 195OC UT WOS:000248420500007 ER PT J AU Guinness, EA Arvidson, RE Jolliff, BL Seelos, KD Seelos, FP Ming, DW Morris, RV Graff, TG AF Guinness, Edward A. Arvidson, Raymond E. Jolliff, Bradley L. Seelos, Kim D. Seelos, Frank P. Ming, Douglas W. Morris, Richard V. Graff, Trevor G. TI Hyperspectral reflectance mapping of cinder cones at the summit of Mauna Kea and implications for equivalent observations on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID IMAGING SPECTROMETER AVIRIS; OMEGA/MARS EXPRESS; REFLECTIVITY SPECTRA; HEMATITE; SPECTROSCOPY; MINERALOGY; HAWAII; ANALOG; SOILS; DUST AB [1] Atmospherically corrected, hyperspectral reflectance data (0.4 to 2.5 mu m) derived from the Airborne Visible Infrared Imaging Spectrometer (AVIRIS), validated with field-based traverses and laboratory analyses, were used to map the distribution of ferric oxide, sulfate, and phyllosilicate minerals exposed on fresh and altered cones on the summit of Mauna Kea Volcano, Hawaii. Spectra from 0.4 to 1.1 mu m exhibit chargeelectronic transition features related to hematite, nanophase iron oxide, and possibly jarosite, whereas spectra from 2.0 to 2.5 mu m are characterized by cation-OH features related to kaolinite, montmorillonite, and saponite. Unaltered cones exhibit concentric zoning of iron oxide signatures with crystalline hematite located near the summits and nanophase iron oxide signatures found at the base of cones and on flow surfaces. Altered cones (Puu Poliahu and Puu Waiau) have exposures of three phyllosilicate and possible jarosite units. In some cases there is zoning with a core of saponite surrounded by montmorillonite. Kaolinite is only found in two exposures on Puu Poliahu with one exposure coinciding with a possible jarosite unit. The relatively small spatial scale associated with alteration zones seen on Mauna Kea demonstrates the importance of obtaining high spatial resolution hyperspectral observations of Mars. C1 Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Guinness, EA (reprint author), Washington Univ, Dept Earth & Planetary Sci, 1 Brookings Dr, St Louis, MO 63130 USA. EM guinness@wunder.wustl.edu RI Seelos, Kimberly/F-4647-2015; Seelos, Frank/C-7875-2016 OI Seelos, Kimberly/0000-0001-7236-0580; Seelos, Frank/0000-0001-9721-941X NR 55 TC 8 Z9 8 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUL 28 PY 2007 VL 112 IS E8 AR E08S11 DI 10.1029/2006JE002822 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 195PW UT WOS:000248425100001 ER PT J AU Burlaga, LF Ness, NF Acuna, MH AF Burlaga, L. F. Ness, N. F. Acuna, M. H. TI Linear magnetic holes in a unipolar region of the heliosheath observed by Voyager 1 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID DRIFT MIRROR INSTABILITY; NONLINEAR ALFVEN WAVES; SOLAR-WIND; MODE STRUCTURES; TERMINATION SHOCK; OBLIQUE SOLITONS; SPACE PLASMAS; FIELD; MAGNETOSHEATH; ULYSSES AB Voyager 1 (V1) observed a unipolar interval in the heliosheath from day of year (DOY) 146-204, 2006, in which the magnetic field B was directed toward the Sun nearly along the spiral field direction. The direction of B was nearly constant in this interval (the 1-sigma fluctuations in the hour averages and 48-s averages of the azimuthal and elevation angles being approximate to +/- 8 degrees and approximate to +/- 5 degrees, respectively). The average magnetic field strength was relatively large, B approximate to 0.21 nT. The fluctuations in both the hour averages and 48-s averages of B were non-Gaussian, being skewed toward small values of B, primarily by the presence of numerous linear magnetic holes. The magnetic holes moved past V1 at a rate of the order of 2/day. The characteristics of nine magnetic holes were analyzed by fitting the magnetic field strength profiles to a Gaussian distribution. The radial extent of the magnetic holes was of the order of 650,000 km, which is approximate to 80 R-L, where R-L is the Larmor radius of the pickup protons in the heliosheath. Although the magnetic holes in the heliosheath are much larger than those at 1 AU, the size in units of R-L is of the same order of magnitude in the two locations, suggesting a common physical nature. C1 NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Planetary Magnetospheres Lab, Greenbelt, MD 20771 USA. Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Code 673, Greenbelt, MD 20771 USA. EM leonard.f.burlaga@nasa.gov NR 67 TC 17 Z9 17 U1 1 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 JUL 27 PY 2007 VL 112 IS A7 AR A07106 DI 10.1029/2007JA012292 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 195QF UT WOS:000248426000006 ER PT J AU De La Haye, V Waite, JH Johnson, RE Yelle, RV Cravens, TE Luhmann, JG Kasprzak, WT Gell, DA Magee, B Leblanc, F Michael, M Jurac, S Robertson, IP AF De la Haye, V. Waite, J. H., Jr. Johnson, R. E. Yelle, R. V. Cravens, T. E. Luhmann, J. G. Kasprzak, W. T. Gell, D. A. Magee, B. Leblanc, F. Michael, M. Jurac, S. Robertson, I. P. TI Cassini Ion and Neutral Mass Spectrometer data in Titan's upper atmosphere and exosphere: Observation of a suprathermal corona SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID NITROGEN; PHOTOCHEMISTRY; IONOSPHERE; ESCAPE; MODEL AB The neutral nitrogen and methane measurements made by Ion and Neutral Mass Spectrometer during Cassini flybys T-A, T-B, and T-5 in Titan's upper atmosphere and exosphere are presented. Large horizontal variations are observed in the total density, recorded to be twice as large during T-A as during T-5. Comparison between the atmospheric and exospheric data show evidence for the presence of a significant population of suprathermal molecules. Using a diffusion model to simultaneously fit the N-2 and CH4 density profiles below 1500 km, the atmospheric structure parameters are determined, taking into account recent changes in the calibration parameters. The best fits are obtained for isothermal profiles with values 152.8 +/- 4.6 K for T-A, 149.0 +/- 9.2 K for T-B, and 157.4 +/- 4.9 K for T-5, suggesting a temperature similar or equal to 5 K warmer at night than at dusk, a trend opposite to that determined by solar-driven models. Using standard exospheric theory and a Maxwellian exobase distribution, a temperature of 20 to 70 K higher would be necessary to fit the T-A, T-B, and egress-T-5 data above 1500 km. The suprathermal component of the corona was fit with various exobase energy distributions, using a method based on the Liouville theorem. This gave a density of suprathermals at the exobase of 4.4 +/- 5.1 x 10(5) cm(-3) and 1.1 +/- 0.9 x 10(5) cm(-3), and an energy deposition rate at the exobase of 1.1 +/- 0.9 x 10(2) eV cm(-3) s(-1) and 3.9 +/- 3.5 x 10(1) eV cm(-3) s(-1) for the hot N-2 and CH4 populations, respectively. The energy deposition rate allowed us to roughly estimate escape rates for nitrogen of similar or equal to 7.7 +/- 7.1 x 10(7) N cm(-2) s(-1) and for methane of similar or equal to 2.8 +/- 2.1 x 10(7) CH4 cm(-2) s(-1). Interestingly, no suprathermal component was observed in the ingress-T-5 data. C1 SW Res Inst, San Antonio, TX 78228 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. IPSL, CNRS, Serv Aeron, F-75252 Paris, France. Indian Inst Technol, Kanpur 208016, Uttar Pradesh, India. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. RP De La Haye, V (reprint author), SW Res Inst, 6220 Culebra Rd, San Antonio, TX 78228 USA. NR 37 TC 62 Z9 62 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 JUL 27 PY 2007 VL 112 IS A7 AR A07309 DI 10.1029/2006JA012222 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 195QF UT WOS:000248426000005 ER PT J AU Brotton, SJ Shapiro, R van der Laan, G Guo, J Glans, PA Ajello, JM AF Brotton, Stephen J. Shapiro, Russell van der Laan, Gerrit Guo, Jinghua Glans, Per-Anders Ajello, Joseph M. TI Valence state fossils in Proterozoic stromatolites by L-edge X-ray absorption spectroscopy SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID BANDED IRON-FORMATIONS; MAGNETIC CIRCULAR-DICHROISM; LAKE-SUPERIOR REGION; MERIDIANI-PLANUM; GUNFLINT FORMATION; MOSSBAUER SPECTROMETER; SEDIMENTARY-ROCKS; HIGH-RESOLUTION; SPIRIT ROVER; GUSEV CRATER AB Paleoproterozioc (ca. 1.9 Ga) stromatolites from the Biwabik Iron-Formation (Minnesota, United States) contain fossil forms which in the literature have been attributed to ancient microbes including iron- oxidising bacteria and cyanobacteria. To search for valence state fossils, we measured Fe3+/Sigma Fe (Sigma Fe = Fe2+ + Fe3+) transverse to the laminae of a Biwabik, probably biogenic stromatolite and compared the results with a scan across the enclosing, likely abiotic sedimentary rock (or interstromatolite fill). To obtain Fe3+/Sigma Fe and information about the site symmetry and crystal field strength, we used L-3 (2p(3/2) -> 3d) soft X-ray absorption spectroscopy and interpreted the measurements using our calculated spectra. We found that Fe3+/Sigma Fe is approximately constant at 0.3 within the stromatolite, increases steeply to around 0.6 in the region of the stromatolite-fill boundary, and then reduces significantly in the interstromatolite fill. The crystal field strength for octahedral Fe3+ increased and became more irregular as the scan moved from the stromatolite into the fill. Our results tentatively suggest that a combination of ancient biological and later diagenetic processes can produce steep gradients in Fe3+/Sigma Fe and alterations in the crystal field strength across a probable abioticbiotic boundary. To describe the L-3 absorption spectra in the stromatolite-fill region, it was necessary to include a significant Fe3+ tetrahedral component, which suggests the presence of magnetite. At other positions, fits using only octahedral Fe2+ and Fe3+ theoretical curves satisfactorily reproduce the spectra. The search for a possible new type of spatial biosignature in the valence state record for ancient stromatolites might help differentiate between the biogenic stromatolites and abiogenic stromatolite-like structures and could even be relevant to the search for fossil evidence of life in extraterrestrial rocks. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Windsor, Dept Phys, Windsor, ON, Canada. Calif State Univ Los Angeles, Geol & Environm Sci, Chico, CA 95928 USA. SERC, Daresbury Lab, Magnet Spect Grp, Warrington WA4 4AD, Cheshire, England. Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester, Lancs, England. Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA USA. Boston Univ, Dept Phys, Boston, MA 02215 USA. RP Brotton, SJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI van der Laan, Gerrit/Q-1662-2015; Glans, Per-Anders/G-8674-2016 OI van der Laan, Gerrit/0000-0001-6852-2495; NR 89 TC 5 Z9 5 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUL 25 PY 2007 VL 112 IS G3 AR G03004 DI 10.1029/2006JG000185 PG 11 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 195PH UT WOS:000248423600001 ER PT J AU Tian, YD Peters-Lidard, CD AF Tian, Yudong Peters-Lidard, Christa D. TI Systematic anomalies over inland water bodies in satellite-based precipitation estimates SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PASSIVE MICROWAVE; RAINFALL ESTIMATION; CLASSIFICATION; ALGORITHMS; RESOLUTION; COVER AB We studied two recent high-resolution precipitation datasets derived from satellite remote-sensing, TRMM 3B42 and CMORPH, and compared them with ground-based radar and gauge measurements in the southeastern U. S.. We found there are systematic differences in rainfall estimates between inland water-body pixels and land pixels. On average, there are about twice as many raining days over water bodies than over land pixels in the satellite products, causing much higher false alarm rates over water bodies. The increased false alarms occur mostly in the form of light rain (< 2 mm/day), and lead to significantly different rain rate distributions between water-body and land pixels. We speculate that this inconsistency is caused by deficiencies in emissivity characterization for the passive microwave-based rainfall retrievals that serve as input to these merged products. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD USA. RP Tian, YD (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM yudong.tian@nasa.gov RI Measurement, Global/C-4698-2015; Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 NR 17 TC 36 Z9 36 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 24 PY 2007 VL 34 IS 14 AR L14403 DI 10.1029/2007GL030787 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 195NU UT WOS:000248419700008 ER PT J AU Fan, JW Zhang, RY Li, GH Tao, WK AF Fan, Jiwen Zhang, Renyi Li, Guohui Tao, Wei-Kuo TI Effects of aerosols and relative humidity on cumulus clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MESOSCALE MODEL MM5; CONVECTIVE CLOUDS; DETAILED MICROPHYSICS; ATMOSPHERIC AEROSOLS; NOX PRODUCTION; DROPLET SIZE; PART II; POLLUTION; RAIN; SIMULATION AB [1]The influences of the aerosol type and concentration and relative humidity ( RH) on cumulus clouds have been investigated using a two-dimensional spectral-bin cloud model. Three simulations are conducted to represent the polluted continental, clean continental, and marine aerosol types. Under the same initial dynamic and thermodynamic conditions, the maritime aerosol case results in more intensive radar reflectivity in both developing and mature stages than the continental aerosol cases, because of enhanced warm rain by collisions and ice processes by deposition growth due to larger droplet sizes and higher supersaturation, respectively. The considerable delay in convective development due to reduced droplet condensation is responsible for the longer cloud lifetime in the marine aerosol case. For the continental case, the most noticeable effects of increasing aerosol number concentrations ( with 15 different initial values) are the increases of the cloud droplet number concentration and cloud water content but a decrease in the effective droplet radius. More latent heat release from increasing condensation results in stronger convection and more melting precipitation at the higher aerosol concentrations. Melting precipitation and secondary clouds primarily contribute to enhanced precipitation with increasing aerosols. The precipitation, however, decreases with increasing aerosol in the extremely high aerosol cases ( over 5 x 10(4) cm(-3)) due to suppression of convection from depleted water vapor and inefficient coalescence. When the initial aerosol concentration exceeds a critical level, most of the cloud properties become less sensitive to aerosols, implying that the aerosol effect on deep convection is more pronounced in relatively clean air than in heavily polluted air. The aerosol effect on the cloud properties is strongly dependent on RH. As the surface RH increases from 40 to 70%, the cloud changes from shallow warm to deep convective types due to a significant increase of convective available potential energy ( CAPE). The aerosol effects on the cloud microphysical properties and precipitation are negligible in dry air ( 40% surface RH), but much more significant in humid air ( 60-70% surface RH). The rain delay is sensitive to RH, but not to aerosols under similar initial thermodynamic conditions. C1 Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fan, JW (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM zhang@ariel.met.tamu.edu RI Zhang, Renyi/A-2942-2011; Fan, Jiwen/E-9138-2011 NR 45 TC 80 Z9 85 U1 2 U2 25 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 24 PY 2007 VL 112 IS D14 AR D14204 DI 10.1029/2006JD008136 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 195OK UT WOS:000248421300002 ER PT J AU Andre, N Persoon, AM Goldstein, J Burch, JL Louarn, P Lewis, GR Rymer, AM Coates, AJ Kurth, WS Sittler, EC Thomsen, MF Crary, FJ Dougherty, MK Gurnett, DA Young, DT AF Andre, N. Persoon, A. M. Goldstein, J. Burch, J. L. Louarn, P. Lewis, G. R. Rymer, A. M. Coates, A. J. Kurth, W. S. Sittler, E. C., Jr. Thomsen, M. F. Crary, F. J. Dougherty, M. K. Gurnett, D. A. Young, D. T. TI Magnetic signatures of plasma-depleted flux tubes in the Saturnian inner magnetosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID DYNAMICS AB Initial Cassini observations have revealed evidence for interchanging magnetic flux tubes in the inner Saturnian magnetosphere. Some of the reported flux tubes differ remarkably by their magnetic signatures, having a depressed or enhanced magnetic pressure relative to their surroundings. The ones with stronger fields have been interpreted previously as either outward moving mass-loaded or inward moving plasma-depleted flux tubes based on magnetometer observations only. We use detailed multi-instrumental observations of small and large density depletions in the inner Saturnian magnetosphere from Cassini Rev. A orbit that enable us to discriminate amongst the two previous and opposite interpretations. Our analysis undoubtedly confirms the similar nature of both types of reported interchanging magnetic flux tubes, which are plasma-depleted, whatever their magnetic signatures are. Their different magnetic signature is clearly an effect associated with latitude. These Saturnian plasma-depleted flux tubes ultimately may play a similar role as the Jovian ones. C1 European Space Agcy, ESTEC, Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. SW Res Inst, San Antonio, TX 78238 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Ctr Etud Spatiales Rayonnements, F-31028 Toulouse, France. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Andre, N (reprint author), European Space Agcy, ESTEC, Sci Support Dept, SCI SM Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands. EM nandre@rssd.esa.int RI Coates, Andrew/C-2396-2008; OI Coates, Andrew/0000-0002-6185-3125; Kurth, William/0000-0002-5471-6202 FU Science and Technology Facilities Council [PP/D00084X/1] NR 19 TC 30 Z9 30 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 21 PY 2007 VL 34 IS 14 AR L14108 DI 10.1029/2007GL030374 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 193PA UT WOS:000248285300006 ER PT J AU Hebb, L Petro, L Ford, HC Ardila, DR Toledo, I Minniti, D Golimowski, DA Clampin, M AF Hebb, Leslie Petro, Larry Ford, Holland C. Ardila, David R. Toledo, Ignacio Minniti, Dante Golimowski, David A. Clampin, Mark TI A search for planets transiting the M-dwarf debris disc host, AU Microscopii SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; stars : individual : AU Mic; stars : late-type; planetary systems; stars : pre-main-sequence ID NEARBY YOUNG STARS; LOW-MASS STARS; CIRCUMSTELLAR DISK; EXTRASOLAR PLANETS; BETA-PICTORIS; DUST DISK; MODELS; SPECTROSCOPY; DISCOVERY AB We present high-cadence, high-precision multiband photometry of the young, MlVe, debris disc star, AU Microscopii. The data were obtained in three continuum filters spanning a wavelength range from 4500 to 6600 A, plus H alpha, over 28 nights in 2005. The light curves show intrinsic stellar variability due to star-spots with an amplitude in the blue band of 0.051 mag and a period of 4.847 d. In addition, three large flares were detected in the data which all occur near the minimum brightness of the star. We remove the intrinsic stellar variability and combine the light curves of all the filters in order to search for transits by possible planetary companions orbiting in the plane of the nearly edge-on debris disc. The combined final light curve has a sampling of 0.35 min and a standard deviation of 6.8 mmag. We performed Monte Carlo simulations by adding fake transits to the observed light curve and find with 95 per cent significance that there are no Jupiter mass planets orbiting in the plane of the debris disc on circular orbits with periods, P <= 5 d. In addition, there are no young Neptune like planets (with radii 2.5 times smaller than the young Jupiter) on circular orbits with periods, P <= 3 d. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hebb, L (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM leslie.hebb@st-andrews.ac.uk RI Clampin, mark/D-2738-2012; OI Toledo, Ignacio/0000-0003-1653-9468; Petro, Larry/0000-0001-8879-528X NR 33 TC 12 Z9 12 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2007 VL 379 IS 1 BP 63 EP 72 DI 10.1111/j.1365-2966.2007.11904.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194WF UT WOS:000248373800007 ER PT J AU Dickinson, C Davies, RD Bronfman, L Casassus, S Davis, RJ Pearson, TJ Readhead, ACS Wilkinson, PN AF Dickinson, C. Davies, R. D. Bronfman, L. Casassus, S. Davis, R. J. Pearson, T. J. Readhead, A. C. S. Wilkinson, P. N. TI CBI limits on 31 GHz excess emission in southern HII regions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms : thermal; ISM : clouds; HII regions; radio continuum : ISM ID MICROWAVE-ANISOTROPY-PROBE; COSMIC BACKGROUND IMAGER; H-II REGIONS; INTERSTELLAR-MEDIUM EMISSION; RECOMBINATION LINE EMISSION; COSMOSOMAS EXPERIMENT; CARINA NEBULA; SPINNING DUST; POLARIZATION OBSERVATIONS; MOSAIC OBSERVATIONS AB We have mapped four regions of the southern Galactic plane at 31 GHz with the Cosmic Background Imager. From the maps, we have extracted the flux densities for six of the brightest H it regions in the southern sky and compared them with multifrequency data from the literature. The fitted spectral index for each source was found to be close to the theoretical value expected for optically thin free-free emission, thus confirming that the majority of flux at 31 GHz is due to free-free emission from ionized gas with an electron temperature of approximate to 7000-8000 K. We also found that, for all six sources, the 31-GHz flux density was slightly higher than the predicted value from data in the literature. This excess emission could be due to spinning dust or another emission mechanism. Comparisons with 100-mu m data indicate an average dust emissivity of 3.3 +/- 1.7 mu K (MJy sr(-1))(-1), or a 95 per cent confidence limit of <6.1 mu K (MJy sr(-1))(-1). This is lower than that found in diffuse clouds at high Galactic latitudes by a factor of similar to 3-4. The most significant detection (3.3 sigma) was found in G284.3-0.3 (RCW 49) and may account for up to approximate to 30 per cent of the total flux density observed at 31 GHz. Here, the dust emissivity of the excess emission is 13.6 +/- 4.2 mu K (MJy sr(-1))(-1) and is within the range observed at high Galactic latitudes. Low-level polarized emission was observed in all six sources with polarization fractions in the range 0.3-0.6 per cent. This is likely to be mainly due to instrumental leakage and is therefore an upper limit to the free-free polarization. It corresponds to an upper limit of similar to 1 per cent for the polarization of anomalous emission. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Chajnantor Observ, Pasadena, CA 91125 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Univ Chile, Dept Astron, Santiago, Chile. RP Dickinson, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-327, Pasadena, CA 91109 USA. EM Clive.Dickinson@jpl.nasa.gov RI Bronfman, Leonardo/H-9544-2013; Pearson, Timothy/N-2376-2015; Casassus, Simon/I-8609-2016 OI Bronfman, Leonardo/0000-0002-9574-8454; Pearson, Timothy/0000-0001-5213-6231; NR 61 TC 36 Z9 36 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2007 VL 379 IS 1 BP 297 EP 307 DI 10.1111/j.1365-2966.2007.11967.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194WF UT WOS:000248373800033 ER PT J AU Crossfield, IJ Troy, M AF Crossfield, Ian J. Troy, Mitchell TI Segment aberration effects on contrast SO APPLIED OPTICS LA English DT Article ID TELESCOPE; SYSTEMS AB High-contrast imaging, particularly the direct detection of extrasolar planets, is a major science driver for the next generation of telescopes. This science requires the suppression of scattered starlight at extremely high levels and that telescopes be correctly designed today to meet these stringent requirements in the future. The challenge increases in systems with complicated aperture geometries such as obscured, segmented telescopes. Such systems can also require intensive modeling and simulation efforts in order to understand the trade-offs between different optical parameters. The feasibility and development of a contrast prediction tool for use in the design and systems engineering of these telescopes is described. The performance of a particular starlight suppression system on a large segmented telescope is described analytically. These analytical results and the results of a contrast predictor are then compared with the results of a full wave-optics simulation. (c) 2007 Optical Society of America. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP Crossfield, IJ (reprint author), CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Ian.J.Crossfield@jpl.nasa.gov NR 15 TC 4 Z9 4 U1 0 U2 0 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 JUL 20 PY 2007 VL 46 IS 21 BP 4533 EP 4540 DI 10.1364/AO.46.004533 PG 8 WC Optics SC Optics GA 191NR UT WOS:000248138500001 PM 17609697 ER PT J AU Keppel-Aleks, G Toon, GC Wennberg, PO Deutscher, NM AF Keppel-Aleks, Gretchen Toon, Geoffrey C. Wennberg, Paul O. Deutscher, Nicholas M. TI Reducing the impact of source brightness fluctuations on spectra obtained by Fourier-transform spectrometry SO APPLIED OPTICS LA English DT Article AB We present a method to reduce the impact of source brightness fluctuations (SBFs) on spectra recorded by Fourier-transform spectrometry (FTS). Interferograms are recorded without AC coupling of the detector signal (DC mode). The SBF are determined by low-pass filtering of the DC interferograms, which are then reweighted by the low-pass, smoothed signal. Atmospheric solar absorption interferograms recorded in DC mode have been processed with and without this technique, and we demonstrate its efficacy in producing more consistent retrievals of atmospheric composition. We show that the reweighting algorithm improves retrievals from interferograms subject to both gray and nongray intensity fluctuations, making the algorithm applicable to atmospheric data contaminated by significant amounts of aerosol or cloud cover. (c) 2007 Optical Society of America. C1 CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. Univ Wollongong, Wollongong, NSW 2522, Australia. RP Keppel-Aleks, G (reprint author), CALTECH, 1200 E California Blvd, Pasadena, CA 91125 USA. EM gka@gps.caltech.edu RI Wennberg, Paul/A-5460-2012; Keppel-Aleks, Gretchen/A-3239-2013; Deutscher, Nicholas/E-3683-2015 OI Deutscher, Nicholas/0000-0002-2906-2577 NR 6 TC 38 Z9 39 U1 1 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JUL 20 PY 2007 VL 46 IS 21 BP 4774 EP 4779 DI 10.1364/AO.46.004774 PG 6 WC Optics SC Optics GA 191NR UT WOS:000248138500030 PM 17609726 ER PT J AU Fukumura, K Kazanas, D AF Fukumura, Keigo Kazanas, Demosthenes TI Accretion disk illumination in Schwarzschild and Kerr geometries: Fitting formulae SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; black hole physics; galaxies : individual (MCG-6-30-15) line : profiles; stars : neutron ID ACTIVE GALACTIC NUCLEI; X-RAY REFLECTION; BLACK-HOLE; LINE-PROFILES; IRON LINE; STRONG GRAVITY; SUZAKU OBSERVATIONS; COLD MATTER; EMISSION; MCG-6-30-15 AB We describe the methodology and compute the illumination of geometrically thin accretion disks around black holes of arbitrary spin parameter a exposed to the radiation of a pointlike isotropic source at arbitrary height above the disk on its symmetry axis. We then provide analytic fitting formulae for the illumination as a function of the source height h and the black hole angular momentum a. We find that for a source on the disk symmetry axis and with h/M > 3, the main effect of the parameter a is allowing the disk to extend to smaller radii (approaching r/M -> 1 as a/M -> 1) and thus allowing the illumination of regions of much higher rotational velocity and redshift. We also compute the illumination profiles for anisotropic emission associated with the motion of the source relative to the accretion disk and present the fractions of photons absorbed by the black hole, intercepted by the disk, or escaping to infinity for both isotropic and anisotropic emission for a/M = 0 and 0.99. As the anisotropy (of a source approaching the disk) increases, the illumination profile reduces (approximately) to a single power law, whose index q, because of absorption of the beamed photons by the black hole, saturates to a value no higher than q >= 3. Finally, we compute the fluorescent Fe line profiles associated with the specific illumination and compare them among various cases. C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Fukumura, K (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 663, Greenbelt, MD 20771 USA. EM fukumura@milkyway.gsfc.nasa.gov; Demos.Kazanas-1@nasa.gov RI XRAY, SUZAKU/A-1808-2009 NR 31 TC 12 Z9 12 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2007 VL 664 IS 1 BP 14 EP 25 DI 10.1086/518883 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 189QA UT WOS:000248002400003 ER PT J AU Dudik, RP Weingartner, JC Satyapal, S Fischer, J Dudley, CC O'Halloran, B AF Dudik, R. P. Weingartner, J. C. Satyapal, S. Fischer, Jacqueline Dudley, C. C. O'Halloran, B. TI Mid-infrared fine-structure line ratios in active galactic nuclei observed with the Spitzer IRS: Evidence for extinction by the torus SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : active; galaxies : starburst; infrared : galaxies; X-rays : galaxies ID ULTRALUMINOUS INFRARED GALAXIES; HUBBLE-SPACE-TELESCOPE; SEYFERT 2 GALAXIES; X-RAY; EMISSION-LINE; CENTAURUS-A; NGC 1365; XMM-NEWTON; STAR-FORMATION; ENERGY-DISTRIBUTIONS AB We present the first systematic investigation of the [Ne v] (14 mu m/24 mu m) and [S III] (18 mu m/33 mu m) infrared line flux ratios, traditionally used to estimate the density of the ionized gas, in a sample of 41 type 1 and type 2 active galactic nuclei (AGNs) observed with the Infrared Spectrograph on board Spitzer. The majority of galaxies with both [Ne v] lines detected have observed [Ne v] line flux ratios consistent with or below the theoretical low-density limit, based on calculations using currently available collision strengths and ignoring absorption and stimulated emission. We find that type 2 AGNs have lower line flux ratios than type 1 AGNs and that all of the galaxies with line flux ratios below the low-density limit are type 2 AGNs. We argue that differential infrared extinction to the [Ne v] emitting region due to dust in the obscuring torus is responsible for the ratios below the low-density limit and we suggest that the ratio may be a tracer of the inclination angle of the torus to our line of sight. Because the temperature of the gas, the amount of extinction, and the effect of absorption and stimulated emission on the line ratios are all unknown, we are not able to determine the electron densities associated with the [ Ne v] line flux ratios for the objects in our sample. We also find that the [S III] emission from the galaxies in our sample is extended and originates primarily in star-forming regions. Since the emission from low-ionization species is extended, any analysis using line flux ratios from such species obtained from slits of different sizes is invalid for most nearby galaxies. C1 George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Greenbelt, MD 20711 USA. USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. RP Dudik, RP (reprint author), George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. NR 147 TC 36 Z9 36 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2007 VL 664 IS 1 BP 71 EP 87 DI 10.1086/518685 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 189QA UT WOS:000248002400008 ER EF