FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Testa, P De Pontieu, B Martinez-Sykora, J DeLuca, E Hansteen, V Cirtain, J Winebarger, A Golub, L Kobayashi, K Korreck, K Kuzin, S Walsh, R DeForest, C Title, A Weber, M AF Testa, Paola De Pontieu, Bart Martinez-Sykora, Juan DeLuca, Ed Hansteen, Viggo Cirtain, Jonathan Winebarger, Amy Golub, Leon Kobayashi, Ken Korreck, Kelly Kuzin, Sergey Walsh, Robert DeForest, Craig Title, Alan Weber, Mark TI OBSERVING CORONAL NANOFLARES IN ACTIVE REGION MOSS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: corona; Sun: magnetic topology; Sun: transition region; Sun: UV radiation ID X-RAY CORONA; TRANSITION REGION; HOT PLASMA; SOLAR CORONA; MAGNETIC RECONNECTION; IMAGING SPECTROMETER; LOOPS OBSERVATIONS; EMISSION; DYNAMICS; HINODE AB The High-resolution Coronal Imager (Hi-C) has provided Fe XII 193 angstrom images of the upper transition region moss at an unprecedented spatial (similar to 0 ''.3-0 ''.4) and temporal (5.5 s) resolution. The Hi-C observations show in some moss regions variability on timescales down to similar to 15 s, significantly shorter than the minute-scale variability typically found in previous observations of moss, therefore challenging the conclusion of moss being heated in a mostly steady manner. These rapid variability moss regions are located at the footpoints of bright hot coronal loops observed by the Solar Dynamics Observatory/Atmospheric Imaging Assembly in the 94 angstrom channel, and by the Hinode/X-Ray Telescope. The configuration of these loops is highly dynamic, and suggestive of slipping reconnection. We interpret these events as signatures of heating events associated with reconnection occurring in the overlying hot coronal loops, i.e., coronal nanoflares. We estimate the order of magnitude of the energy in these events to be of at least a few 10(23) erg, also supporting the nanoflare scenario. These Hi-C observations suggest that future observations at comparable high spatial and temporal resolution, with more extensive temperature coverage, are required to determine the exact characteristics of the heating mechanism(s). C1 [Testa, Paola; DeLuca, Ed; Golub, Leon; Korreck, Kelly; Weber, Mark] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [De Pontieu, Bart; Martinez-Sykora, Juan; Title, Alan] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, Juan] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Hansteen, Viggo] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Cirtain, Jonathan; Winebarger, Amy; Kobayashi, Ken] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Kuzin, Sergey] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia. [Walsh, Robert] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England. [DeForest, Craig] Southwest Res Inst, Boulder, CO 80302 USA. RP Testa, P (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM ptesta@cfa.harvard.edu RI Kuzin, Sergey/M-3435-2015; DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Golub, Leon/0000-0001-9638-3082 FU Lockheed-Martin [SP02H1701R]; NASA [NNM07AB07C, NNX08BA99G, NNX08AH45G, NNX11AN98G] FX We thank the referees for their useful comments which greatly helped to improve the Letter. P.T. was supported by contract SP02H1701R from Lockheed-Martin, and NASA contract NNM07AB07C to SAO. B.D.P. was supported through NASA grants NNX08BA99G, NNX08AH45G, and NNX11AN98G. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ, NASA, and STFC (UK) as partners, and operated by these agencies in cooperation with ESA and NSC (Norway). NR 50 TC 39 Z9 39 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2013 VL 770 IS 1 AR UNSP L1 DI 10.1088/2041-8205/770/1/L1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 155CR UT WOS:000319723500001 ER PT J AU Eckstein, MP Mack, SC Liston, DB Bogush, L Menzel, R Krauzlis, RJ AF Eckstein, Miguel P. Mack, Stephen C. Liston, Dorion B. Bogush, Lisa Menzel, Randolf Krauzlis, Richard J. TI Rethinking human visual attention: Spatial cueing effects and optimality of decisions by honeybees, monkeys and humans SO VISION RESEARCH LA English DT Article DE Visual attention; Computational modeling; Posner cueing paradigm; Human monkey bee psychophysics; Bayesian ideal observer ID SIGNAL-DETECTION-THEORY; LEARNING SITUATION; APIS-MELLIFERA; SEARCH; PROBABILITY; BEHAVIOR; UNCERTAINTY; PERCEPTION; MODELS; CUES AB Visual attention is commonly studied by using visuo-spatial cues indicating probable locations of a target and assessing the effect of the validity of the cue on perceptual performance and its neural correlates. Here, we adapt a cueing task to measure spatial cueing effects on the decisions of honeybees and compare their behavior to that of humans and monkeys in a similarly structured two-alternative forced-choice perceptual task. Unlike the typical cueing paradigm in which the stimulus strength remains unchanged within a block of trials, for the monkey and human studies we randomized the contrast of the signal to simulate more real world conditions in which the organism is uncertain about the strength of the signal. A Bayesian ideal observer that weights sensory evidence from cued and uncued locations based on the cue validity to maximize overall performance is used as a benchmark of comparison against the three animals and other suboptimal models: probability matching, ignore the cue, always follow the cue, and an additive bias/single decision threshold model. We find that the cueing effect is pervasive across all three species but is smaller in size than that shown by the Bayesian ideal observer. Humans show a larger cueing effect than monkeys and bees show the smallest effect. The cueing effect and overall performance of the honeybees allows rejection of the models in which the bees are ignoring the cue, following the cue and disregarding stimuli to be discriminated, or adopting a probability matching strategy. Stimulus strength uncertainty also reduces the theoretically predicted variation in cueing effect with stimulus strength of an optimal Bayesian observer and diminishes the size of the cueing effect when stimulus strength is low. A more biologically plausible model that includes an additive bias to the sensory response from the cued location, although not mathematically equivalent to the optimal observer for the case stimulus strength uncertainty, can approximate the benefits of the more computationally complex optimal Bayesian model. We discuss the implications of our findings on the field's common conceptualization of covert visual attention in the cueing task and what aspects, if any, might be unique to humans. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Eckstein, Miguel P.; Mack, Stephen C.] Univ Calif Santa Barbara, Dept Psychol & Brain Sci, Santa Barbara, CA 93106 USA. [Liston, Dorion B.] San Jose State Univ, San Jose, CA 95192 USA. [Liston, Dorion B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bogush, Lisa; Menzel, Randolf] Free Univ Berlin, Dept Biol, Berlin, Germany. [Krauzlis, Richard J.] NEI, Sensorimotor Res Lab, NIH, Bethesda, MD 20892 USA. RP Eckstein, MP (reprint author), Univ Calif Santa Barbara, Dept Psychol & Brain Sci, Vis & Image Understanding Lab, Santa Barbara, CA 93106 USA. EM eckstein@psych.ucsb.edu; mack@psych.ucsb.edu; dorion.b.liston@nasa.gov; bogusch@neurobiologie.fu-berlin.de; menzel@neurobiologie.fu-berlin.de; richard.krauzlis@nih.gov FU NEI NIH HHS [R01 EY015925] NR 76 TC 8 Z9 8 U1 2 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0042-6989 J9 VISION RES JI Vision Res. PD JUN 7 PY 2013 VL 85 SI SI BP 5 EP 19 DI 10.1016/j.visres.2012.12.011 PG 15 WC Neurosciences; Ophthalmology SC Neurosciences & Neurology; Ophthalmology GA 171CU UT WOS:000320903500002 PM 23298793 ER PT J AU Fuller, TL Thomassen, HA Peralvo, M Buermann, W Mila, B Kieswetter, CM Jarrin-V, P Devitt, SEC Mason, E Schweizer, RM Schlunegger, J Chan, J Wang, O Schneider, CJ Pollinger, JP Saatchi, S Graham, CH Wayne, RK Smith, TB AF Fuller, Trevon L. Thomassen, Henri A. Peralvo, Manuel Buermann, Wolfgang Mila, Borja Kieswetter, Charles M. Jarrin-, Pablo, V Devitt, Susan E. Cameron Mason, Eliza Schweizer, Rena M. Schlunegger, Jasmin Chan, Janice Wang, Ophelia Schneider, Christopher J. Pollinger, John P. Saatchi, Sassan Graham, Catherine H. Wayne, Robert K. Smith, Thomas B. TI Intraspecific morphological and genetic variation of common species predicts ranges of threatened ones SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE biodiversity; conservation planning; indicator species; reserve selection; surrogacy ID RAIN-FOREST BIRD; CONSERVATION PRIORITIES; ECOLOGICAL GRADIENTS; CLIMATE-CHANGE; SOUTH-AMERICA; DIVERSITY; BIODIVERSITY; PATTERNS; ECUADOR; AREA AB Predicting where threatened species occur is useful for making informed conservation decisions. However, because they are usually rare, surveying threatened species is often expensive and time intensive. Here, we show how regions where common species exhibit high genetic and morphological divergence among populations can be used to predict the occurrence of species of conservation concern. Intraspecific variation of common species of birds, bats and frogs from Ecuador were found to be a significantly better predictor for the occurrence of threatened species than suites of environmental variables or the occurrence of amphibians and birds. Fully 93 per cent of the threatened species analysed had their range adequately represented by the geographical distribution of the morphological and genetic variation found in seven common species. Both higher numbers of threatened species and greater genetic and morphological variation of common species occurred along elevation gradients. Higher levels of intraspecific divergence may be the result of disruptive selection and/or introgression along gradients. We suggest that collecting data on genetic and morphological variation in common species can be a cost effective tool for conservation planning, and that future biodiversity inventories include surveying genetic and morphological data of common species whenever feasible. C1 [Fuller, Trevon L.; Thomassen, Henri A.; Buermann, Wolfgang; Mila, Borja; Pollinger, John P.; Saatchi, Sassan; Smith, Thomas B.] Univ Calif Los Angeles, Ctr Trop Res Inst Environm & Sustainabil, Los Angeles, CA 90095 USA. [Thomassen, Henri A.] Consorcio Desarrollo Sostenible Ecorreg Andina, Iniciativa Estudios Ambient, Quito, Ecuador. [Buermann, Wolfgang] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Mila, Borja] CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. [Kieswetter, Charles M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Jarrin-, Pablo, V] Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Yasuni Res Stn, Quito, Ecuador. [Devitt, Susan E. Cameron] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Mason, Eliza; Schweizer, Rena M.; Schlunegger, Jasmin; Chan, Janice; Pollinger, John P.; Wayne, Robert K.; Smith, Thomas B.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Mason, Eliza] Univ N Carolina, Sch Med, Dept Microbiol & Immunol, Chapel Hill, NC 27599 USA. [Wang, Ophelia] Univ Texas Austin, Dept Geog & Environm, Austin, TX 78712 USA. [Wang, Ophelia] Univ Arizona, Ctr Sustainable Environm, Flagstaff, AZ 86011 USA. [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Graham, Catherine H.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. RP Fuller, TL (reprint author), Univ Calif Los Angeles, Ctr Trop Res Inst Environm & Sustainabil, La Kretz Hall,Suite 300,619 Charles E Young Dr Ea, Los Angeles, CA 90095 USA. EM fullertl@ucla.edu RI Cameron Devitt, Susan/E-2659-2013; Fuller, Trevon/B-8087-2014; Graham, Catherine/A-9560-2011; OI Mila, Borja/0000-0002-6446-0079 FU NSF [IRCEB9977072]; NASA [IDS/03-0169-0347, NNG05GB37G] FX We thank R. Calsbeek, R. Harrigan, B. Larison, R. E. Ricklefs, three reviewers and Associate Editor Daniel Rabosky for comments that improved the manuscript. This work was supported by NSF grant no. IRCEB9977072 to T. B. S, R. K. W. and C.J.S.; and NASA grant nos IDS/03-0169-0347 to T. B. S., R. K. W., and C.J.S.; and NNG05GB37G to C.H.G. NR 58 TC 1 Z9 2 U1 1 U2 67 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUN 7 PY 2013 VL 280 IS 1760 AR 20130423 DI 10.1098/rspb.2013.0423 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 131VH UT WOS:000318024600013 PM 23595273 ER PT J AU Horikawa, DD Cumbers, J Sakakibara, I Rogoff, D Leuko, S Harnoto, R Arakawa, K Katayama, T Kunieda, T Toyoda, A Fujiyama, A Rothschild, LJ AF Horikawa, Daiki D. Cumbers, John Sakakibara, Iori Rogoff, Dana Leuko, Stefan Harnoto, Raechel Arakawa, Kazuharu Katayama, Toshiaki Kunieda, Takekazu Toyoda, Atsushi Fujiyama, Asao Rothschild, Lynn J. TI Analysis of DNA Repair and Protection in the Tardigrade Ramazzottius varieornatus and Hypsibius dujardini after Exposure to UVC Radiation SO PLOS ONE LA English DT Article ID MILNESIUM-TARDIGRADUM; RICHTERSIUS-CORONIFER; THYMINE DIMERS; NEW-MODEL; TOLERANCE; RESISTANCE; PHOTOLYASE; SPORES; VIVO AB Tardigrades inhabiting terrestrial environments exhibit extraordinary resistance to ionizing radiation and UV radiation although little is known about the mechanisms underlying the resistance. We found that the terrestrial tardigrade Ramazzottius varieornatus is able to tolerate massive doses of UVC irradiation by both being protected from forming UVC-induced thymine dimers in DNA in a desiccated, anhydrobiotic state as well as repairing the dimers that do form in the hydrated animals. In R. varieornatus accumulation of thymine dimers in DNA induced by irradiation with 2.5 kJ/m(2) of UVC radiation disappeared 18 h after the exposure when the animals were exposed to fluorescent light but not in the dark. Much higher UV radiation tolerance was observed in desiccated anhydrobiotic R. varieornatus compared to hydrated specimens of this species. On the other hand, the freshwater tardigrade species Hypsibius dujardini that was used as control, showed much weaker tolerance to UVC radiation than R. varieornatus, and it did not contain a putative phrA gene sequence. The anhydrobiotes of R. varieornatus accumulated much less UVC-induced thymine dimers in DNA than hydrated one. It suggests that anhydrobiosis efficiently avoids DNA damage accumulation in R. varieornatus and confers better UV radiation tolerance on this species. Thus we propose that UV radiation tolerance in tardigrades is due to the both high capacities of DNA damage repair and DNA protection, a two-pronged survival strategy. C1 [Horikawa, Daiki D.; Cumbers, John; Rogoff, Dana; Leuko, Stefan; Rothschild, Lynn J.] NASA Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA USA. [Horikawa, Daiki D.; Rothschild, Lynn J.] Brown Univ, NASA Astrobiol Inst, Providence, RI 02912 USA. [Cumbers, John; Rothschild, Lynn J.] Brown Univ, Dept Mol Biol Cell Biol & Biochem, Providence, RI 02912 USA. [Sakakibara, Iori] Inst Cochin Genet Mol, INSERM, U1016, F-75014 Paris, France. [Sakakibara, Iori] CNRS, UMR 8104, Paris, France. [Sakakibara, Iori] Univ Paris 05, Sorbonne Paris Cite, Paris, France. [Harnoto, Raechel] Calif Polytech State Univ San Luis Obispo, San Luis Obispo, CA 93407 USA. [Arakawa, Kazuharu] Keio Univ, Inst Adv Biosci, Fujisawa, Kanagawa, Japan. [Katayama, Toshiaki] Univ Tokyo, Inst Med Sci, Ctr Human Genome, Tokyo, Japan. [Kunieda, Takekazu] Univ Tokyo, Grad Sch Sci, Dept Biol Sci, Tokyo 113, Japan. [Toyoda, Atsushi] Natl Inst Genet, Ctr Informat Biol, Mishima, Shizuoka 411, Japan. [Fujiyama, Asao] Natl Inst Informat, Principles Informat Res Div, Tokyo, Japan. RP Horikawa, DD (reprint author), NASA Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA USA. EM horikawadd@gmail.com; Lynn.J.Rothschild@nasa.gov RI Kunieda, Takekazu/G-4946-2014 FU NASA Ames Research Center; NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the NASA Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. The funder had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 31 TC 15 Z9 15 U1 12 U2 64 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUN 6 PY 2013 VL 8 IS 6 AR e64793 DI 10.1371/journal.pone.0064793 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 173SK UT WOS:000321099000023 PM 23762256 ER PT J AU Stephenson, JD Hallis, LJ Nagashima, K Freeland, SJ AF Stephenson, James D. Hallis, Lydia J. Nagashima, Kazuhide Freeland, Stephen J. TI Boron Enrichment in Martian Clay SO PLOS ONE LA English DT Article ID AQUEOUS ALTERATION; MASS-SPECTROMETRY; WEST GREENLAND; METEORITE; RIBOSE; ADSORPTION; EVOLUTION; CATALYSTS; ISOTOPES; SUGARS AB We have detected a concentration of boron in martian clay far in excess of that in any previously reported extra-terrestrial object. This enrichment indicates that the chemistry necessary for the formation of ribose, a key component of RNA, could have existed on Mars since the formation of early clay deposits, contemporary to the emergence of life on Earth. Given the greater similarity of Earth and Mars early in their geological history, and the extensive disruption of Earth's earliest mineralogy by plate tectonics, we suggest that the conditions for prebiotic ribose synthesis may be better understood by further Mars exploration. C1 [Stephenson, James D.; Hallis, Lydia J.; Freeland, Stephen J.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Hallis, Lydia J.; Nagashima, Kazuhide] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP Stephenson, JD (reprint author), Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. EM jds@ifa.hawaii.edu OI Stephenson, James/0000-0002-6427-5703 FU National Aeronautics and Space Administration through the NASA Astrobiology Institute through the Office of Space Science [NNA09DA77A] FX This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 5 Z9 5 U1 3 U2 20 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUN 6 PY 2013 VL 8 IS 6 AR e64624 DI 10.1371/journal.pone.0064624 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 173SK UT WOS:000321099000009 PM 23762242 ER PT J AU Turner, W AF Turner, Woody CA 14 Co-Signatories TI Satellites: make data freely accessible SO NATURE LA English DT Letter C1 [Turner, Woody] NASA, Div Earth Sci, Washington, DC 20546 USA. RP Turner, W (reprint author), NASA, Div Earth Sci, Washington, DC 20546 USA. EM woody.turner@nasa.gov OI Szantoi, Zoltan/0000-0003-2580-4382 NR 1 TC 8 Z9 8 U1 0 U2 8 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 6 PY 2013 VL 498 IS 7452 BP 37 EP 37 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 158DC UT WOS:000319947800021 PM 23739415 ER PT J AU Hanna, E Navarro, FJ Pattyn, F Domingues, CM Fettweis, X Ivins, ER Nicholls, RJ Ritz, C Smith, B Tulaczyk, S Whitehouse, PL Zwally, HJ AF Hanna, Edward Navarro, Francisco J. Pattyn, Frank Domingues, Catia M. Fettweis, Xavier Ivins, Erik R. Nicholls, Robert J. Ritz, Catherine Smith, Ben Tulaczyk, Slawek Whitehouse, Pippa L. Zwally, H. Jay TI Ice-sheet mass balance and climate change SO NATURE LA English DT Review ID SEA-LEVEL RISE; SATELLITE-GRAVIMETRY; RECONCILED ESTIMATE; RADAR ALTIMETRY; GROUNDING LINES; WATER STORAGE; GREENLAND; SHELF; GLACIERS; MODEL AB Since the 2007 Intergovernmental Panel on Climate Change Fourth Assessment Report, new observations of ice-sheet mass balance and improved computer simulations of ice-sheet response to continuing climate change have been published. Whereas Greenland is losing ice mass at an increasing pace, current Antarctic ice loss is likely to be less than some recently published estimates. It remains unclear whether East Antarctica has been gaining or losing ice mass over the past 20 years, and uncertainties in ice-mass change for West Antarctica and the Antarctic Peninsula remain large. We discuss the past six years of progress and examine the key problems that remain. C1 [Hanna, Edward] Univ Sheffield, Dept Geog, Sheffield S10 2TN, S Yorkshire, England. [Navarro, Francisco J.] Univ Politecn Madrid, Dept Matemat Aplicada Tecnol Informac, E-28040 Madrid, Spain. [Pattyn, Frank] Univ Libre Bruxelles, Lab Glaciol, B-1050 Brussels, Belgium. [Domingues, Catia M.] Univ Tasmania, Antarctic Climate & Ecosyst Cooperat Res Ctr, Aspendale, Vic 3195, Australia. [Fettweis, Xavier] Univ Liege, Dept Geog, B-4000 Liege, Belgium. [Ivins, Erik R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nicholls, Robert J.] Univ Southampton, Fac Engn & Environm, Southampton SO17 1BJ, Hants, England. [Ritz, Catherine] Univ Grenoble 1, CNRS, Lab Glaciol & Geophys Environm, F-38402 St Martin Dheres, France. [Smith, Ben] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA. [Tulaczyk, Slawek] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Whitehouse, Pippa L.] Univ Durham, Dept Geog, Durham DH1 3LE, England. [Zwally, H. Jay] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. RP Hanna, E (reprint author), Univ Sheffield, Dept Geog, Sheffield S10 2TN, S Yorkshire, England. EM ehanna@sheffield.ac.uk RI Navarro, Francisco/L-2941-2014; Domingues, Catia /A-2901-2015; Hanna, Edward/H-2219-2016; Nicholls, Robert/G-3898-2010; OI Whitehouse, Pippa/0000-0002-9092-3444; Pattyn, Frank/0000-0003-4805-5636; Navarro, Francisco/0000-0002-5147-0067; Domingues, Catia /0000-0001-5100-4595; Hanna, Edward/0000-0002-8683-182X; Nicholls, Robert/0000-0002-9715-1109; Fettweis, Xavier/0000-0002-4140-3813 FU International Council for Science (ICSU); SCAR; IASC; WCRP; International Glaciological Society (IGS); International Association of Cryospheric Sciences (IACS); Climate and Cryosphere (CliC); Association of Polar Early Career Scientists (APECS) FX The work presented here is based on the Ice-Sheet Mass Balance and Sea Level (ISMASS) workshop that was held in Portland, Oregon, USA, on 14 July 2012. This workshop was jointly organized by the Scientific Committee on Antarctic Research (SCAR), the International Arctic Science Committee (IASC) and the Word Climate Research Programme (WCRP), and was co-sponsored by the International Council for Science (ICSU), SCAR, IASC, WCRP, the International Glaciological Society (IGS) and the International Association of Cryospheric Sciences (IACS), with support from Climate and Cryosphere (CliC) and the Association of Polar Early Career Scientists (APECS). NR 100 TC 75 Z9 76 U1 11 U2 258 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUN 6 PY 2013 VL 498 IS 7452 BP 51 EP 59 DI 10.1038/nature12238 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 158DC UT WOS:000319947800031 PM 23739423 ER PT J AU Kawai, J Jagota, S Kaneko, T Obayashi, Y Khare, BN McKay, CP Kobayashi, K AF Kawai, Jun Jagota, Seema Kaneko, Takeo Obayashi, Yumiko Khare, Bishun N. McKay, Christopher P. Kobayashi, Kensei TI Titan Tholins as Amino Acid Precursors and Their Solubility in Possible Titan Liquidospheres SO CHEMISTRY LETTERS LA English DT Article ID HIGH-PRESSURE; HAZE; ATMOSPHERE; SIMULATION; CHEMISTRY; AEROSOLS; AMMONIA; SURFACE; GAS AB Experimental simulations have previously shown that tholins (complex solid organics) can be abundantly formed in Titan's atmosphere and that they contain precursors of amino acids. In this study, we investigated their relevance to possible chemical evolution toward the generation of life in various potential Titan environments (liquidospheres), using tholins synthesized by plasma discharge at low pressure (LP, 26 Pa) and high pressure (HP, 133 Pa). We focused our study on composition of amino acids recovered from LP and HP tholins, as well as on the solubility of these tholins in solvents such as hexane, acetonitrile, ethanol, methanol, water, and ammonia water. Both hydrolyzed extracts of LP and HP tholins were composed of a wide variety of amino acids. Tholins were dissolved more easily in polar solvents than in nonpolar ones: Ammonia water, simulating a potential Titan subsurface ocean, could dissolve tholins quite efficiently. These results show thus the possibility of starting chemical evolution toward life's origin in Titan's environment. C1 [Kawai, Jun; Kaneko, Takeo; Obayashi, Yumiko; Kobayashi, Kensei] Yokohama Natl Univ, Grad Sch Chem & Biotechnol, Hodogaya Ku, Yokohama, Kanagawa 2408501, Japan. [Jagota, Seema; Khare, Bishun N.; McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kawai, J (reprint author), Yokohama Natl Univ, Grad Sch Chem & Biotechnol, Hodogaya Ku, 79-5 Tokiwadai, Yokohama, Kanagawa 2408501, Japan. EM kawai-jun-jy@ynu.ac.jp OI Kaneko, Takeo/0000-0002-8904-1030; Kobayashi, Kensei/0000-0003-2951-1341 FU Leave a Nest Co. FX We would like to thank the scientists at NASA Ames Research Center for their cooperation in sample collection. We are also grateful to the members of Yokohama National University for helpful discussions. This research was funded by Leave a Nest Co. NR 22 TC 0 Z9 0 U1 1 U2 23 PU CHEMICAL SOC JAPAN PI TOKYO PA 1-5 KANDA-SURUGADAI CHIYODA-KU, TOKYO, 101-8307, JAPAN SN 0366-7022 EI 1348-0715 J9 CHEM LETT JI Chem. Lett. PD JUN 5 PY 2013 VL 42 IS 6 BP 633 EP 635 DI 10.1246/cl.130101 PG 3 WC Chemistry, Multidisciplinary SC Chemistry GA 174RQ UT WOS:000321173500021 ER PT J AU Morton, DC Le Page, Y DeFries, R Collatz, GJ Hurtt, GC AF Morton, D. C. Le Page, Y. DeFries, R. Collatz, G. J. Hurtt, G. C. TI Understorey fire frequency and the fate of burned forests in southern Amazonia SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE deforestation; fire; feedbacks; climate; land use ID CLIMATE-CHANGE; TROPICAL FORESTS; BRAZILIAN AMAZON; DEFORESTATION; SCENARIOS; WILDFIRES AB Recent drought events underscore the vulnerability of Amazon forests to understorey fires. The long-term impact of fires on biodiversity and forest carbon stocks depends on the frequency of fire damages and deforestation rates of burned forests. Here, we characterized the spatial and temporal dynamics of understorey fires (1999-2010) and deforestation (2001-2010) in southern Amazonia using new satellite-based estimates of annual fire activity (greater than 50 ha) and deforestation (greater than 10 ha). Understorey forest fires burned more than 85 500 km(2) between 1999 and 2010 (2.8% of all forests). Forests that burned more than once accounted for 16 per cent of all understorey fires. Repeated fire activity was concentrated in Mato Grosso and eastern Para, whereas single fires were widespread across the arc of deforestation. Routine fire activity in Mato Grosso coincided with annual periods of low night-time relative humidity, suggesting a strong climate control on both single and repeated fires. Understorey fires occurred in regions with active deforestation, yet the interannual variability of fire and deforestation were uncorrelated, and only 2.6 per cent of forests that burned between 1999 and 2008 were deforested for agricultural use by 2010. Evidence from the past decade suggests that future projections of frontier landscapes in Amazonia should separately consider economic drivers to project future deforestation and climate to project fire risk. C1 [Morton, D. C.; Collatz, G. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Le Page, Y.; Hurtt, G. C.] Joint Global Change Res Inst, College Pk, MD 20740 USA. [DeFries, R.] Columbia Univ, Dept Evolutionary Ecol & Environm Biol, New York, NY USA. [Hurtt, G. C.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. RP Morton, DC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM douglas.morton@nasa.gov RI Morton, Douglas/D-5044-2012; collatz, george/D-5381-2012 FU NASA; US Department of Energy Office of Science Integrated Assessment Program FX This study was supported by the NASA Terrestrial Ecology and Interdisciplinary Science Programs and the US Department of Energy Office of Science Integrated Assessment Program. NR 33 TC 43 Z9 43 U1 3 U2 51 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD JUN 5 PY 2013 VL 368 IS 1619 SI SI AR 20120163 DI 10.1098/rstb.2012.0163 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 130LQ UT WOS:000317918900007 PM 23610169 ER PT J AU DeLeon-Rodriguez, N Lathem, TL Rodriguez-R, LM Barazesh, JM Anderson, BE Beyersdorf, AJ Ziemba, LD Bergin, M Nenes, A Konstantinidis, KT AF DeLeon-Rodriguez, Natasha Lathem, Terry L. Rodriguez-R, Luis M. Barazesh, James M. Anderson, Bruce E. Beyersdorf, Andreas J. Ziemba, Luke D. Bergin, Michael Nenes, Athanasios Konstantinidis, Konstantinos T. TI Reply to Smith and Griffin: Methods, air flows, and conclusions are robust in the DeLeon-Rodriguez et al. study SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID AIRBORNE C1 [DeLeon-Rodriguez, Natasha; Rodriguez-R, Luis M.; Konstantinidis, Konstantinos T.] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. [Lathem, Terry L.; Bergin, Michael; Nenes, Athanasios] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Barazesh, James M.; Bergin, Michael; Konstantinidis, Konstantinos T.] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. [Nenes, Athanasios] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. [Anderson, Bruce E.; Beyersdorf, Andreas J.; Ziemba, Luke D.] NASA, Chem & Dynam Branch, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. RP Nenes, A (reprint author), Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. EM athanasios.nenes@gatech.edu; kostas@ce.gatech.edu RI Beyersdorf, Andreas/N-1247-2013; Barazesh, James/L-5680-2013; OI Rodriguez-R, Luis M/0000-0001-7603-3093 NR 6 TC 2 Z9 2 U1 0 U2 15 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 JUN 4 PY 2013 VL 110 IS 23 BP E2085 EP E2085 DI 10.1073/pnas.1304466110 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 165SD UT WOS:000320503000002 PM 23882709 ER PT J AU Smith, DJ Griffin, DW AF Smith, David Joseph Griffin, Dale Warren TI Inadequate methods and questionable conclusions in atmospheric life study SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Smith, David Joseph] NASA, Surface Syst Off, Kennedy Space Ctr, FL 32899 USA. [Griffin, Dale Warren] US Geol Survey, Coastal & Marine Sci Ctr, St Petersburg, FL 33701 USA. RP Smith, DJ (reprint author), NASA, Surface Syst Off, Kennedy Space Ctr, FL 32899 USA. EM david.j.smith-3@nasa.gov NR 3 TC 4 Z9 4 U1 0 U2 11 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 JUN 4 PY 2013 VL 110 IS 23 BP E2084 EP E2084 DI 10.1073/pnas.1302612110 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 165SD UT WOS:000320503000001 PM 23633574 ER PT J AU Vasileiou, V Jacholkowska, A Piron, F Bolmont, J Couturier, C Granot, J Stecker, FW Cohen-Tanugi, J Longo, F AF Vasileiou, V. Jacholkowska, A. Piron, F. Bolmont, J. Couturier, C. Granot, J. Stecker, F. W. Cohen-Tanugi, J. Longo, F. TI Constraints on Lorentz invariance violation from Fermi-Large Area Telescope observations of gamma-ray bursts SO PHYSICAL REVIEW D LA English DT Article ID LOOP QUANTUM-GRAVITY; HIGH-ENERGY; SPACE-TELESCOPE; CPT VIOLATION; GRB 090926A; COMPONENT; TESTS; DISPERSION; AFTERGLOW; EMISSION AB We analyze the MeV/GeV emission from four bright gamma-ray bursts (GRBs) observed by the Fermi Large Area Telescope to produce robust, stringent constraints on a dependence of the speed of light in vacuo on the photon energy (vacuum dispersion), a form of Lorentz invariance violation (LIV) allowed by some quantum gravity (QG) theories. First, we use three different and complementary techniques to constrain the total degree of dispersion observed in the data. Additionally, using a maximally conservative set of assumptions on possible source-intrinsic, spectral-evolution effects, we constrain any vacuum dispersion solely attributed to LIV. We then derive limits on the QG energy scale (the energy scale where LIV-inducing QG effects become strong, E-QG) and the coefficients of the Standard Model Extension. For the subluminal case (where high-energy photons propagate more slowly than lower-energy photons) and without taking into account any source-intrinsic dispersion, our most stringent limits (at 95% C. L.) are obtained from GRB 090510 and are E-QG,E-1 > 7: 6 times the Planck energy (E-Pl) and E-QG,E-2 > 1.3 x 10(11) GeV for linear and quadratic leading-order LIV-induced vacuum dispersion, respectively. These limits improve the latest constraints by Fermi and H. E. S. S. by a factor of similar to 2. Our results disfavor any class of models requiring E-QG,E-1 less than or similar to E-Pl. C1 [Vasileiou, V.; Piron, F.; Cohen-Tanugi, J.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3,CC 72, F-34095 Montpellier 5, France. [Jacholkowska, A.; Bolmont, J.; Couturier, C.] Univ Paris 07, Univ Paris 06, Lab Phys Nucl & Hautes Energies, CNRS,IN2P3, F-75252 Paris 5, France. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Stecker, F. W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Stecker, F. W.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. RP Vasileiou, V (reprint author), Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3,CC 72, Pl Eugene Bataillon, F-34095 Montpellier 5, France. EM vlasisva@gmail.com; agnieszka.jacholkowska@cern.ch RI Couturier, Camille/K-7585-2013 OI Couturier, Camille/0000-0002-0168-1106 NR 67 TC 39 Z9 40 U1 0 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD JUN 4 PY 2013 VL 87 IS 12 AR UNSP 122001 DI 10.1103/PhysRevD.87.122001 PG 31 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 157RX UT WOS:000319917900001 ER PT J AU Klatt, CG Inskeep, WP Herrgard, MJ Jay, ZJ Rusch, DB Tringe, SG Parenteau, MN Ward, DM Boomer, SM Bryant, DA Miller, SR AF Klatt, Christian G. Inskeep, William P. Herrgard, Markus J. Jay, Zackary J. Rusch, Douglas B. Tringe, Susannah G. Parenteau, M. Niki Ward, David M. Boomer, Sarah M. Bryant, Donald A. Miller, Scott R. TI Community structure and function of high-temperature chlorophototrophic microbial mats inhabiting diverse geothermal environments SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE microbial mats; microbial interactions; phototrophic bacteria; functional genomics; thermophilic bacteria ID YELLOWSTONE-NATIONAL-PARK; BLUE-GREEN-ALGAE; CANDIDATUS CHLORACIDOBACTERIUM THERMOPHILUM; CYANOBACTERIUM MASTIGOCLADUS-LAMINOSUS; PHOTOTROPHIC FE(II) OXIDATION; ALKALINE HOT-SPRINGS; CHLOROFLEXUS-AURANTIACUS; SULFIDEQUINONE OXIDOREDUCTASE; SOFTWARE ENVIRONMENT; NONSULFUR BACTERIA AB Six phototrophic microbial mat communities from different geothermal springs (YNP) were studied using metagenome sequencing and geochemical analyses. The primary goals of this work were to determine differences in community composition of high-temperature phototrophic mats distributed across the Yellowstone geothermal ecosystem, and to identify metabolic attributes of predominant organisms present in these communities that may correlate with environmental attributes important in niche differentiation. Random shotgun metagenome sequences from six phototrophic communities (average similar to 53 Mbp/site) were subjected to multiple taxonomic, phylogenetic, and functional analyses. All methods, including G + C content distribution, MEGAN analyses, and oligonucleotide frequency-based clustering, provided strong support for the dominant community members present in each site. Cyanobacteria were only observed in non-sulfidic sites; de novo assemblies were obtained for Synechococcus-like populations at Chocolate Pots (CP_7) and Fischerella-like populations at White Creek (WC_6). Chloroflexi-like sequences (esp. Rosei-flexus and/or Chloroflexus spp.) were observed in all six samples and contained genes involved in bacteriochlorophyll biosynthesis and the 3-hydroxypropionate carbon fixation pathway. Other major sequence assemblies were obtained for a Chlorobiales population from CP_7 (proposed family Thermochlorobacteriaceae), and an anoxygenic, sulfur-oxidizing Thermochromatium-like (Gamma-proteobacteria) population from Bath Lake Vista Annex (BLVA_20). Additional sequence coverage is necessary to establish more complete assemblies of other novel bacteria in these sites (e.g., Bacteroidetes and Firmicutes); however, current assemblies suggested that several of these organisms play important roles in heterotrophic and fermentative metabolisms. Definitive linkages were established between several of the dominant phylotypes present in these habitats and important functional processes such as photosynthesis, carbon fixation, sulfur oxidation, and fermentation. C1 [Klatt, Christian G.; Inskeep, William P.; Jay, Zackary J.; Ward, David M.] Montana State Univ, Dept Land Resources & Environm Sci, Bozeman, MT 59717 USA. [Klatt, Christian G.; Inskeep, William P.; Jay, Zackary J.; Ward, David M.] Montana State Univ, Thermal Biol Inst, Bozeman, MT 59717 USA. [Herrgard, Markus J.] Tech Univ Denmark, Novo Nordisk Fdn Ctr Biosustainabil, Horsholm, Denmark. [Rusch, Douglas B.] Indiana Univ, Ctr Genom & Bioinformat, Bloomington, IN USA. [Tringe, Susannah G.] Joint Genome Inst, Dept Energy, Walnut Creek, CA USA. [Parenteau, M. Niki] Search Extraterr Intelligence Inst, Mountain View, CA USA. [Parenteau, M. Niki] NASA, Ames Res Ctr, Mountain View, CA USA. [Boomer, Sarah M.] Western Oregon Univ, Monmouth, OR USA. [Bryant, Donald A.] Penn State Univ, Dept Biochem & Mol Biol, University Pk, PA 16802 USA. [Bryant, Donald A.] Montana State Univ, Dept Chem & Biochem, Bozeman, MT 59717 USA. [Miller, Scott R.] Univ Montana, Dept Biol Sci, Missoula, MT USA. RP Inskeep, WP (reprint author), Montana State Univ, Bozeman, MT 59717 USA. EM binskeep@montana.edu OI Tringe, Susannah/0000-0001-6479-8427 FU National Science Foundation Research Coordination Network Program [MCB 0342269]; DOE-Joint Genome Institute Community Sequencing Program [CSP 787081]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; YNP metagenome project [YELL-5568] FX Authors appreciate support from the National Science Foundation Research Coordination Network Program (MCB 0342269), the DOE-Joint Genome Institute Community Sequencing Program (CSP 787081) as well as all individual author institutions and associated research support that together has made this study possible. The work conducted by the U.S. Department of Energy Joint Genome Institute is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Authors appreciate research permitting focused on the YNP metagenome project (Permit No, YELL-5568, 2007-2010), and managed by C. Hendrix and S. Guenther (Center for Resources, YNP). NR 105 TC 24 Z9 25 U1 5 U2 40 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD JUN 3 PY 2013 VL 4 AR 106 DI 10.3389/fmicb.2013.00106 PG 23 WC Microbiology SC Microbiology GA AA5US UT WOS:000331165700001 PM 23761787 ER PT J AU Prasad, NS Pliutau, D AF Prasad, Narasimha S. Pliutau, Denis TI Cross-band relative absorption technique for the measurement of molecular mixing ratios SO OPTICS EXPRESS LA English DT Article ID SPECTROSCOPIC DATABASE; ATMOSPHERIC CO2; LIDAR AB We describe a new method for the measurement of molecular mixing ratios called Cross-Band Relative Absorption (CoBRA). The proposed method is based on relative measurements in different molecular bands referenced to a band of O-2 with properly selected wavelength combinations providing high level of cancelation in temperature sensitivities. The CoBRA approach is particularly promising for satellite based remote sensing of molecular mixing ratios of the atmospheric trace gases. Very low temperature sensitivities and the potential of achieving close weighting function matching for the measurement and reference wavelengths are the main advantages of the method. The effectiveness of CoBRA approach is demonstrated for the retrieval of CO2 mixing ratios (XCO2) with application to the ASCENDS mission. (C) 2013 Optical Society of America C1 [Prasad, Narasimha S.; Pliutau, Denis] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Prasad, NS (reprint author), NASA, Langley Res Ctr, MS 468, Hampton, VA 23681 USA. EM narasimha.s.prasad@nasa.gov FU Earth Science Technology Office (ESTO); NASA FX This study was supported by the Earth Science Technology Office (ESTO), and the NASA Postdoctoral Program (NPP) administered by Oak Ridge Associated Universities. NR 15 TC 0 Z9 0 U1 1 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUN 3 PY 2013 VL 21 IS 11 BP 13279 EP 13292 DI 10.1364/OE.21.013279 PG 14 WC Optics SC Optics GA 156II UT WOS:000319814900032 PM 23736581 ER PT J AU Balin, Y Kaul, B Kokhanenko, G Winker, D AF Balin, Yury Kaul, Bruno Kokhanenko, Grigorii Winker, David TI Transformation of light backscattering phase matrices of crystal clouds depending on the zenith sensing angle SO OPTICS EXPRESS LA English DT Article ID ORIENTED ICE PLATES; CIRRUS CLOUDS; PARTICLE ORIENTATION; LIDAR; SCATTERING; DEPOLARIZATION AB Problems encountered in the interpretation of results of laser sensing of crystal clouds are considered. The parameters characterizing the cloud particle orientation are determined through the backscattering phase matrix elements. It is demonstrated how these parameters are related to the probability density of particle distribution over the spatial orientation angles. Trends in the change of the backscattering phase matrices attendant to variations of the zenith sensing angle are shown on the example of a monodisperse ice particle ensemble. (C) 2013 Optical Society of America C1 [Balin, Yury; Kaul, Bruno; Kokhanenko, Grigorii] Russian Acad Sci, Inst Atmospher Opt, Siberian Branch, Tomsk 634055, Russia. [Winker, David] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Balin, Y (reprint author), Russian Acad Sci, Inst Atmospher Opt, Siberian Branch, Tomsk 634055, Russia. EM kokh@iao.ru FU Russian Foundation for Basic Research [13-05-00096-a]; Ministry of Education and Science [11.519.11.6033, 14.518.11.7063]; CRDF [RUGI-7053-TO-11] FX This work was supported in part by the Russian Foundation for Basic Research (grant No. 13-05-00096-a), the Ministry of Education and Science (State Contracts Nos. 11.519.11.6033 and 14.518.11.7063), and CRDF grant RUGI-7053-TO-11. NR 30 TC 1 Z9 2 U1 0 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUN 3 PY 2013 VL 21 IS 11 BP 13408 EP 13418 DI 10.1364/OE.21.013408 PG 11 WC Optics SC Optics GA 156II UT WOS:000319814900044 PM 23736593 ER PT J AU Park, Y Choi, SH AF Park, Yeonjoon Choi, Sang H. TI Miniaturization of optical spectroscopes into Fresnel microspectrometers SO JOURNAL OF NANOPHOTONICS LA English DT Article DE microspectrometer; Fresnel diffraction grating; gradient grating; ring grating ID NANO-IMPRINT LITHOGRAPHY; FOURIER-TRANSFORM SPECTROSCOPY; SMALL-F-NUMBER; FOCUSED-ION; STRAY-LIGHT; INFRARED SPECTROMETERS; PLASMON RESONANCE; ZONE PLATES; BEAM; FABRICATION AB Miniaturized optical instruments have become very important in industry as smart phones and tablet PCs increase in popularity. A chronology of spectrometer development shows that a simple numerical point of view affords important insights. A tiny spectrometer, which is smaller than a few millimeters size, cannot easily rely on the conventional Fraunhofer diffraction due to its optical criterion limit. As an alternate solution to build smaller spectrometers, a Fresnel spectrometer chip with a gradient line grating is attractive. The fabricated Fresnel spectrometers have optical path volumes of about 1 mm(3) and spectral resolutions of 10 to 23 nm. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. C1 [Park, Yeonjoon] Natl Inst Aerosp, Hampton, VA 23666 USA. [Choi, Sang H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Park, Y (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM Sang.H.Choi@NASA.gov FU NASA, USA [SAA-15546]; Gacheon University of Medicine and Science under KOSEF program by the Ministry of Science, Technology, and Education, Republic of Korea FX This research was supported by the space act agreement SAA-15546 of NASA, USA and Gacheon University of Medicine and Science under KOSEF program by the Ministry of Science, Technology, and Education, Republic of Korea. NR 102 TC 4 Z9 5 U1 2 U2 15 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1934-2608 J9 J NANOPHOTONICS JI J. Nanophotonics PD JUN 3 PY 2013 VL 7 AR 077599 DI 10.1117/1.JNP.7.077599 PG 18 WC Nanoscience & Nanotechnology; Optics SC Science & Technology - Other Topics; Optics GA 156CD UT WOS:000319797100001 ER PT J AU Ojha, R AF Ojha, Roopesh TI Parsec-scale structure of quasars: dawn of the golden age? SO BULLETIN OF THE ASTRONOMICAL SOCIETY OF INDIA LA English DT Article DE galaxies: quasars: general; galaxies: nuclei; galaxies: jets; radio continuation: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; COMPACT SYMMETRIC OBJECTS; BASE-LINE ARRAY; EXTRAGALACTIC RADIO-SOURCES; HEMISPHERE ICRF SOURCES; EGRET-DETECTED QUASARS; BL LACERTAE OBJECTS; VLBI OBSERVATIONS AB Half a century after their discovery, the study of quasars remains one of the most fascinating intellectual challenges in astronomy. Quasars are laboratories for everything from relativity to magnetohydrodynamics and are perhaps the best available probes for cosmology. A tremendous amount has been learned about quasars and yet many of the most fundamental questions about their physics remain open. Parsec-scale observations have played an indispensable role in building up our current understanding of quasars; virtually everything we know about quasars depends on such observations. However, the finest hour for parsec scale observations may be just beginning. This is partly due to the development of highly reliable VLBI networks (which is continuing) but mostly due to the unprecedented availability of multiepoch, simultaneous, broadband observations that have long been the 'holy grail' for quasar researchers. C1 [Ojha, Roopesh] NASA Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20770 USA. [Ojha, Roopesh] Catholic Univ Amer, Washington, DC 20064 USA. RP Ojha, R (reprint author), NASA Goddard Space Flight Ctr, Astroparticle Phys Lab, Code 661, Greenbelt, MD 20770 USA. EM Roopesh.Ojha@nasa.gov FU NASA [NNH10ZDA001N]; NASA Postdoctoral Program at the Goddard Space Flight Center FX The author gratefully acknowledges his colleagues in the TANAMI and Fermi/LAT programs from whom he continues to learn. The author sincerely apologizes for the vast range of wonderful work that he was unable to touch upon in such a brief review. This research was funded in part by NASA through Fermi Guest Investigator grant NNH10ZDA001N (proposal number 41213). This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This research has made use of NASA's Astrophysics Data System. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the SIMBAD database (operated at CDS, Strasbourg, France). NR 112 TC 1 Z9 1 U1 0 U2 1 PU INDIAN INST ASTROPHYSICS PI BANGALORE PA G C ANUPAMA EDITOR, BANGALORE, 560 034, INDIA SN 0304-9523 J9 B ASTRON SOC INDIA JI Bull. Astron. Soc. India. PD JUN PY 2013 VL 41 IS 2 BP 117 EP 136 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1UK UT WOS:000333755700001 ER PT J AU Peters, BT Brady, RA Batson, CD Guined, JR Ploutz-Snyder, RJ Mulavara, AP Bloomberg, JJ AF Peters, Brian T. Brady, Rachel A. Batson, Crystal D. Guined, Jamie R. Ploutz-Snyder, Robert J. Mulavara, Ajitkumar P. Bloomberg, Jacob J. TI Adaptation in Locomotor Stability, Cognition, and Metabolic Cost During Sensory Discordance SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE human locomotion; sensory discordance; instability; perturbation; gait adaptation ID SPACE SUIT BIOENERGETICS; TREADMILL WALKING; EFFICIENCY; SPACEFLIGHT; STRATEGIES; CLEARANCE; TASK AB Background: Locomotor instability may affect planetary extravehicular activities during the initial adaptation to the new gravitational environment. The goal of this study was to quantify the locomotor, cognitive, and metabolic effects of exposure to a discordant sensory environment. Methods: A treadmill mounted on a 6-degree-of-freedom motion base was used to present 15 healthy subjects with a destabilizing support surface while they walked. Dependent measures of locomotor stability, cognitive load, and metabolic cost were stride frequency (SF), reaction time (RT), and the volume of oxygen consumed (VO2), respectively. Subjects completed an 8-min baseline walk followed by 20 min of walking with a continuous, sinusoidal, laterally oscillating support-surface perturbation. Data for minutes 1, 7, 13, and 20 of the support-surface perturbation period were compared with the baseline. Results: SF, RT, and VO2 were significantly greater during support-surface motion than during the baseline walking condition and showed a trend toward recovery to baseline levels during the perturbation period. Results demonstrated that adaptation to walking in a discordant sensory environment has quantifiable and significant costs in SF, RT, and VO2 as shown by mean increases of 9%, 20%, and 4%, respectively, collected during the first minute of exposure. By the fourth minute of exposure, mean VO2 consumption had increased to 20% over its baseline. Discussion: We believe that preflight sensorimotor adaptation training paradigms will impart gains in stability and the ability to multitask, and might increase productive mission time by extending work time in extravehicular activity suits where metabolic expenditure is a limiting factor. C1 [Peters, Brian T.; Brady, Rachel A.; Batson, Crystal D.; Guined, Jamie R.; Ploutz-Snyder, Robert J.; Mulavara, Ajitkumar P.; Bloomberg, Jacob J.] NASA, Johnson Space Ctr, Houston, TX USA. RP Peters, BT (reprint author), Wyle Sci Technol & Engn Grp, 1290 Hercules Dr,Suite 120, Houston, TX 77058 USA. EM brian.peters-1@nasa.gov FU National Space Biomedical Research Institute through NASA [NCC 9-58] FX This work was supported by the National Space Biomedical Research Institute through NASA NCC 9-58. None of the authors have any financial or personal relationships with other people or organizations that could inappropriately influence this work. NR 29 TC 0 Z9 0 U1 1 U2 3 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD JUN PY 2013 VL 84 IS 6 BP 567 EP 572 DI 10.3357/ASEM.3529.2013 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AD1LS UT WOS:000332996100003 PM 23745284 ER PT J AU Southern, T Roberts, DP Moiseev, N Ross, A Kim, JH AF Southern, Theodore Roberts, Dustyn P. Moiseev, Nikolay Ross, Amy Kim, Joo H. TI Space Suit Glove Design with Advanced Metacarpal Phalangeal Joints and Robotic Hand Evaluation SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE pressurized glove garment; space suit; robotic hand testing; anthropometric; biomimetic design; neutral configuration; stiffness; torque ID PROSTHESIS AB Background: One area of space suits that is ripe for innovation is the glove. Existing models allow for some fine motor control, but the power grip-the act of grasping a bar-is cumbersome due to high torque requirements at the knuckle or metacarpal phalangeal joint (MCP). This area in particular is also a major source of complaints of pain and injury as reported by astronauts. Method: This paper explores a novel fabrication and patterning technique that allows for more freedom of movement and less pain at this crucial joint in the manned space suit glove. The improvements are evaluated through unmanned testing, manned testing while depressurized in a vacuum glove box, and pressurized testing with a robotic hand. Results: MCP joint flex score improved from 6 to 6.75 (out of 10) in the final glove relative to the baseline glove, and torque required for flexion decreased an average of 17% across all fingers. Qualitative assessments during unpressurized and depressurized manned testing also indicated the final glove was more comfortable than the baseline glove. Discussion: The quantitative results from both human subject questionnaires and robotic torque evaluation suggest that the final iteration of the glove design enables flexion at the MCP joint with less torque and more comfort than the baseline glove. C1 Final Frontier Design, Brooklyn, NY USA. [Kim, Joo H.] NYU, Polytech Inst, Dept Mech & Aerosp Engn, Brooklyn, NY USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Kim, JH (reprint author), NYU, Polytech Inst, Dept Mech & Aerosp Engn, Brooklyn, NY USA. EM jhkim@poly.edu RI Kim, Joo/I-9517-2012 FU U.S. National Aeronautics and Space Administration (NASA) under Phase I SBIR [NNX11CG24P]; National Science Foundation Graduate Research Fellowship [DGE-1104522] FX This research was supported in part by the U.S. National Aeronautics and Space Administration (NASA) under Phase I SBIR grant NNX11CG24P and by a National Science Foundation Graduate Research Fellowship to D. Roberts under Grant No. DGE-1104522. NR 20 TC 0 Z9 0 U1 1 U2 7 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD JUN PY 2013 VL 84 IS 6 BP 633 EP 638 DI 10.3357/ASEM.3531.2013 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AD1LS UT WOS:000332996100013 PM 23745294 ER PT J AU Nguyen, N AF Nhan Nguyen TI Least-Squares Model-Reference Adaptive Control with Chebyshev Orthogonal Polynomial Approximation SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article ID NEURAL-NETWORKS; ROBUSTNESS; DYNAMICS AB This paper presents a model-reference adaptive control approach for systems with unstructured uncertainty based on two least-squares parameter estimation methods: gradient-based method and recursive least-squares method. The unstructured uncertainty is approximated by Chebyshev orthogonal polynomial basis functions. The use of orthogonal basis functions improves the function approximation significantly and enables better convergence of parameter estimates. The least-squares gradient adaptive control achieves superior parameter convergence as compared to the standard model-reference adaptive control. Flight control simulations were conducted with four adaptive controllers: least-squares gradient adaptive control, recursive least-squares adaptive control, standard model-reference adaptive control, and neural-network adaptive control. The results show that the recursive least-squares adaptive control achieves better robustness as measured by a time-delay margin, while the least-squares gradient adaptive control achieves better tracking performance than both the standard model-reference adaptive control and neural-network adaptive control. C1 NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Nguyen, N (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. EM nhan.t.nguyen@nasa.gov NR 28 TC 2 Z9 2 U1 0 U2 8 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD JUN PY 2013 VL 10 IS 6 BP 268 EP 286 DI 10.2514/1.I010037 PG 19 WC Engineering, Aerospace SC Engineering GA AB2FV UT WOS:000331609500002 ER PT J AU Doelling, DR Loeb, NG Keyes, DF Nordeen, ML Morstad, D Nguyen, C Wielicki, BA Young, DF Sun, MG AF Doelling, David R. Loeb, Norman G. Keyes, Dennis F. Nordeen, Michele L. Morstad, Daniel Nguyen, Cathy Wielicki, Bruce A. Young, David F. Sun, Moguo TI Geostationary Enhanced Temporal Interpolation for CERES Flux Products SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID ENERGY SYSTEM INSTRUMENT; ANGULAR-DISTRIBUTION MODELS; METEOROLOGICAL SATELLITE IMAGERS; RADIATION BUDGET; PART I; RAPID CALIBRATION; TERRA SATELLITE; CLOUDS; METHODOLOGY; CHANNELS AB The Clouds and the Earth's Radiant Energy System (CERES) instruments on board the Terra and Aqua spacecraft continue to provide an unprecedented global climate record of the earth's top-of-atmosphere (TOA) energy budget since March 2000. A critical step in determining accurate daily averaged flux involves estimating the flux between CERES Terra or Aqua overpass times. CERES employs the CERES-only (CO) and the CERES geostationary (CG) temporal interpolation methods. The CO method assumes that the cloud properties at the time of the CERES observation remain constant and that it only accounts for changes in albedo with solar zenith angle and diurnal land heating, by assuming a shape for unresolved changes in the diurnal cycle. The CG method enhances the CERES data by explicitly accounting for changes in cloud and radiation between CERES observation times using 3-hourly imager data from five geostationary (GEO) satellites. To maintain calibration traceability, GEO radiances are calibrated against Moderate Resolution Imaging Spectroradiometer (MODIS) and the derived GEO fluxes are normalized to the CERES measurements. While the regional (1 degrees latitude x 1 degrees longitude) monthly-mean difference between the CG and CO methods can exceed 25 W m(-2) over marine stratus and land convection, these regional biases nearly cancel in the global mean. The regional monthly CG shortwave (SW) and longwave (LW) flux uncertainty is reduced by 20%, whereas the daily uncertainty is reduced by 50% and 20%, respectively, over the CO method, based on comparisons with 15-min Geostationary Earth Radiation Budget (GERB) data. C1 [Doelling, David R.; Loeb, Norman G.; Wielicki, Bruce A.; Young, David F.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Keyes, Dennis F.; Nordeen, Michele L.; Morstad, Daniel; Nguyen, Cathy; Sun, Moguo] SSAI, Hampton, VA USA. RP Doelling, DR (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM david.r.doelling@nasa.gov FU NASA CERES project FX This work has been funded by the NASA CERES project. The products and the validation could not have been accomplished without the help of the CERES TISA team. The authors also thank the CERES, GERB, Megha-Tropiques, and CLARREO science teams for their insightful temporal averaging discussions. These data were obtained from the NASA Langley Research Center EOSDIS Distributed Active Archive Center. NR 31 TC 54 Z9 55 U1 0 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD JUN PY 2013 VL 30 IS 6 BP 1072 EP 1090 DI 10.1175/JTECH-D-12-00136.1 PG 19 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 301EF UT WOS:000330514900004 ER PT J AU Rose, FG Rutan, DA Charlock, T Smith, GL Kato, S AF Rose, Fred G. Rutan, David A. Charlock, Thomas Smith, G. Louis Kato, Seiji TI Algorithm for the Constraining of Radiative Transfer Calculations to CERES-Observed Broadband Top-of-Atmosphere Irradiance SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID ENERGY SYSTEM INSTRUMENT; ANGULAR-DISTRIBUTION MODELS; BOUNDARY-LAYER CLOUDS; AEROSOL RETRIEVALS; FLUX ALGORITHMS; TERRA SATELLITE; SURFACE ALBEDO; VALIDATION; PARAMETERIZATION; METHODOLOGY AB NASA's Clouds and the Earth's Radiant Energy System (CERES) project is responsible for operation and data processing of observations from scanning radiometers on board the Tropical Rainfall Measuring Mission (TRMM), Terra, Aqua, and Suomi National Polar-Orbiting Partnership (NPP) satellites. The clouds and radiative swath (CRS) CERES data product contains irradiances computed using a radiative transfer model for nearly all CERES footprints in addition to top-of-atmosphere (TOA) irradiances derived from observed radiances by CERES instruments. This paper describes a method to constrain computed irradiances by CERES-derived TOA irradiances using Lagrangian multipliers. Radiative transfer model inputs include profiles of atmospheric temperature, humidity, aerosols and ozone, surface temperature and albedo, and up to two sets of cloud properties for a CERES footprint. Those inputs are adjusted depending on predefined uncertainties to match computed TOA and CERES-derived TOA irradiance. Because CERES instantaneous irradiances for an individual footprint also include uncertainties, primarily due to the conversion of radiance to irradiance using anisotropic directional models, the degree of the constraint depends on CERES-derived TOA irradiance as well. As a result of adjustment, TOA computed-minus-observed standard deviations are reduced from 8 to 4 W m(-2) for longwave irradiance and from 15 to 6 W m(-2) for shortwave irradiance. While agreement of computed TOA with CERES-derived irradiances improves, comparisons with surface observations show that model constrainment to the TOA does not reduce computation bias error at the surface. After constrainment, shortwave down at the surface has an increased bias (standard deviation) of 1% (0.5%) and longwave increases by 0.2% (0.1%). Clear-sky changes are negligible. C1 [Rose, Fred G.; Rutan, David A.; Smith, G. Louis] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Charlock, Thomas; Kato, Seiji] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. RP Rutan, DA (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. EM david.a.rutan@nasa.gov OI Rose, Fred G/0000-0003-0769-0772 NR 52 TC 6 Z9 6 U1 1 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD JUN PY 2013 VL 30 IS 6 BP 1091 EP 1106 DI 10.1175/JTECH-D-12-00058.1 PG 16 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 301EF UT WOS:000330514900005 ER PT J AU Meneghini, R Liao, L AF Meneghini, Robert Liao, Liang TI Modified Hitschfeld-Bordan Equations for Attenuation-Corrected Radar Rain Reflectivity: Application to Nonuniform Beamfilling at Off-Nadir Incidence SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID TRMM PRECIPITATION RADAR; PATH-INTEGRATED ATTENUATION; SURFACE REFERENCE TECHNIQUE; SPACEBORNE RADAR; PROFILING ALGORITHM; SINGLE-FREQUENCY; RETRIEVAL; AIRBORNE AB As shown by Takahashi et al., multiple path attenuation estimates over the field of view of an airborne or spaceborne weather radar are feasible for off-nadir incidence angles. This follows from the fact that the surface reference technique, which provides path attenuation estimates, can be applied to each radar range gate that intersects the surface. This study builds on this result by showing that three of the modified Hitschfeld-Bordan estimates for the attenuation-corrected radar reflectivity factor can be generalized to the case where multiple path attenuation estimates are available, thereby providing a correction to the effects of nonuniform beamfilling. A simple simulation is presented showing some strengths and weaknesses of the approach. C1 [Meneghini, Robert] NASA, GSFC, Greenbelt, MD 20771 USA. [Liao, Liang] Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA. [Liao, Liang] Morgan State Univ, Greenbelt, MD USA. RP Meneghini, R (reprint author), NASA, GSFC, Code 612, Greenbelt, MD 20771 USA. EM robert.meneghini-1@nasa.gov FU NASA headquarters under NASA's Precipitation Measurement Mission Program [NNH09ZDA001N-PRECIP] FX This work is supported by Dr. Ramesh Kakar of NASA headquarters under NASA's Precipitation Measurement Mission Program NNH09ZDA001N-PRECIP. NR 19 TC 7 Z9 7 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD JUN PY 2013 VL 30 IS 6 BP 1149 EP 1160 DI 10.1175/JTECH-D-12-00192.1 PG 12 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 301EF UT WOS:000330514900009 ER PT J AU Yu, LY Leckey, CAC AF Yu, Lingyu Leckey, Cara A. C. TI Lamb wave-based quantitative crack detection using a focusing array algorithm SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES LA English DT Article DE Focusing array imaging; crack detection; Lamb waves; finite integration; simulation; elastodynamic finite integration technique; piezoelectric wafer sensors ID WAFER ACTIVE SENSORS; FINITE INTEGRATION TECHNIQUE; PLATE STRUCTURES; DAMAGE DETECTION; TRANSDUCER ARRAYS; TIME-REVERSAL; LARGE AREAS; INSPECTION; IDENTIFICATION; SCATTERING AB Cracks are common defects in aluminum plate-like components that are in widespread use in aerospace, shipbuilding, and other industries. Ultrasonic detection using Lamb waves has proven to be an efficient method for crack detection and localization. However, quantitative information regarding crack size or orientation is of paramount importance for damage diagnosis and life prediction. In this article, employing a sparsely arranged piezoelectric sensor array, a quantitative crack detection and imaging approach using a Lamb wave-focusing array algorithm is developed and presented. Additionally, Lamb wave propagation on thin-wall plates and wave interaction with crack damage was studied using three-dimensional elastodynamic finite integration technique. The focusing array imaging algorithm was then developed and applied to both simulation and experimental data to generate intensity images of the structure under interrogation. Experimentally, wafer-type piezoelectric actuators/sensors are permanently installed on the testing structure to generate Lamb waves as well as to measure the waves propagating through the structures. Our results show that when applied to either experimental or simulated data, the focusing array algorithms yield images containing quantitative damage information. The results also demonstrate that three-dimensional elastodynamic finite integration technique can be used for future simulation-based investigations of sensing optimization for various damage scenarios. C1 [Yu, Lingyu] Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA. [Leckey, Cara A. C.] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23665 USA. RP Yu, LY (reprint author), Univ S Carolina, Dept Mech Engn, 300 Main St,RM A111, Columbia, SC 29208 USA. EM yu3@cec.sc.edu FU South Carolina Research Foundation (SCRF) [SAA1-1181]; National Aeronautics and Space Administration (NASA) Langley research center [SAA1-1181] FX This work was conducted in part through the non-reimbursement space act umbrella agreement SAA1-1181 between the South Carolina Research Foundation (SCRF) and the National Aeronautics and Space Administration (NASA) Langley research center. NR 49 TC 13 Z9 13 U1 2 U2 18 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1045-389X EI 1530-8138 J9 J INTEL MAT SYST STR JI J. Intell. Mater. Syst. Struct. PD JUN PY 2013 VL 24 IS 9 BP 1138 EP 1152 DI 10.1177/1045389X12469452 PG 15 WC Materials Science, Multidisciplinary SC Materials Science GA 298KZ UT WOS:000330324100011 ER PT J AU Ivins, ER James, TS Wahr, J Schrama, EJO Landerer, FW Simon, KM AF Ivins, Erik R. James, Thomas S. Wahr, John Schrama, Ernst J. O. Landerer, Felix W. Simon, Karen M. TI Antarctic contribution to sea level rise observed by GRACE with improved GIA correction SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE Antarctica; sea level rise; ice sheet mass balance; GRACE; GIA models; mantle viscosity ID GLACIAL ISOSTATIC-ADJUSTMENT; ICE-AGE EARTH; WEST ANTARCTICA; EAST ANTARCTICA; GRAVITY-FIELD; MASS-BALANCE; DEGLACIAL HISTORY; EXPOSURE AGES; UPLIFT RATES; SHEET AB Antarctic volume changes during the past 21 thousand years are smaller than previously thought, and here we construct an ice sheet history that drives a forward model prediction of the glacial isostatic adjustment (GIA) gravity signal. The new model, in turn, should give predictions that are constrained with recent uplift data. The impact of the GIA signal on a Gravity Recovery and Climate Experiment (GRACE) Antarctic mass balance estimate depends on the specific GRACE analysis method used. For the method described in this paper, the GIA contribution to the apparent surface mass change is re-evaluated to be +5513 Gt/yr by considering a revised ice history model and a parameter search for vertical motion predictions that best fit the GPS observations at 18 high-quality stations. Although the GIA model spans a range of possible Earth rheological structure values, the data are not yet sufficient for solving for a preferred value of upper and lower mantle viscosity nor for a preferred lithospheric thickness. GRACE monthly solutions from the Center for Space Research Release 04 (CSR-RL04) release time series from January 2003 to the beginning of January 2012, uncorrected for GIA, yield an ice mass rate of +2.9 29 Gt/yr. The new GIA correction increases the solved-for ice mass imbalance of Antarctica to -5734 Gt/yr. The revised GIA correction is smaller than past GRACE estimates by about 50 to 90 Gt/yr. The new upper bound to the sea level rise from the Antarctic ice sheet, averaged over the time span 2003.0-2012.0, is about 0.160.09 mm/yr. C1 [Ivins, Erik R.; Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [James, Thomas S.; Simon, Karen M.] Geol Survey Canada, Sidney, BC, Canada. [James, Thomas S.; Simon, Karen M.] Univ Victoria, Sch Earth & Ocean Sci, Victoria, BC, Canada. [Wahr, John] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Wahr, John] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Schrama, Ernst J. O.] Delft Univ Technol, Fac Aerosp Engn, Delft, Netherlands. RP Ivins, ER (reprint author), CALTECH, Jet Prop Lab, MS 300-233,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM erik.r.ivins@jpl.nasa.gov OI Landerer, Felix/0000-0003-2678-095X FU NASA's Earth Science Division; NASA [NNX08AF02G, NNXI0AR66G]; NASA's Making Earth Science Data Records for Use in Research Environments (MEaSUREs) program; ArcticNet Networks of Centres of Excellence FX The research support for E.R.I. and F.W.L. comes from NASA's Earth Science Division with grants from both the Cryosphere Program and the Earth Surface and Interior Focus Area as part of the GRACE Science Team effort. The work of E.R.I. and F.W.L. was performed at the Jet Propulsion Laboratory, California Institute of Technology. J.W. was partially supported by NASA grants NNX08AF02G and NNXI0AR66G and by NASA's Making Earth Science Data Records for Use in Research Environments (MEaSUREs) program. Robert Briggs is thanked for discussions and for providing data from his PhD Thesis. We thank Geruo A for calculating the ICE-5G VM2 GIA responses and three anonymous reviewers for thorough and helpful reviews. This is also a contribution of the Climate Change Geoscience Program of the Earth Sciences Sector (ESS) of Natural Resources Canada. T.S.J. and K.S. gratefully acknowledge support from the ArcticNet Networks of Centres of Excellence. The authors acknowledge Paul Wessel and the University of Hawaii for General Mapping Tools [Wessel and Smith, 1998]. This is ESS contribution 20120237. NR 95 TC 53 Z9 58 U1 4 U2 36 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD JUN PY 2013 VL 118 IS 6 BP 3126 EP 3141 DI 10.1002/jgrb.50208 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 295LW UT WOS:000330118600031 ER PT J AU Lin, YNN Sladen, A Ortega-Culaciati, F Simons, M Avouac, JP Fielding, EJ Brooks, BA Bevis, M Genrich, J Rietbrock, A Vigny, C Smalley, R Socquet, A AF Lin, Yu-nung Nina Sladen, Anthony Ortega-Culaciati, Francisco Simons, Mark Avouac, Jean-Philippe Fielding, Eric J. Brooks, Benjamin A. Bevis, Michael Genrich, Jeff Rietbrock, Andreas Vigny, Christophe Smalley, Robert Socquet, Anne TI Coseismic and postseismic slip associated with the 2010 Maule Earthquake, Chile: Characterizing the Arauco Peninsula barrier effect SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE postseismic deformation; seismic cycle; finite fault model; rate-and-state friction; barrier effect; Arauco Peninsula ID SUMATRA-ANDAMAN EARTHQUAKE; TOKACHI-OKI EARTHQUAKE; INTERSEISMIC STRAIN ACCUMULATION; SPACE-TIME DISTRIBUTION; SOUTH-CENTRAL CHILE; SANRIKU-HARUKA-OKI; SUBDUCTION ZONE; FAULT SLIP; JAPAN TRENCH; SEISMIC GAP AB Observations of coseismic and postseismic deformation associated with the 2010 Mw=8.8 Maule earthquake in south-central Chile provide constraints on the spatial heterogeneities of frictional properties on a major subduction megathrust and how they have influenced the seismic rupture and postseismic effects. We find that the bulk of coseismic slip occurs within a single elongated patch approximately 460 km long and 100 km wide between the depths of 15 and 40km. We infer three major patches of afterslip: one extends northward along strike and downdip of the major coseismic patch between 40 and 60km depth; the other two bound the northern and southern ends of the coseismic patch. The southern patch offshore of the Arauco Peninsula is the only place showing resolvable afterslip shallower than 20 km depth. Estimated slip potency associated with postseismic slip in the 1.3years following the earthquake amounts to 20-30% of that generated coseismically. Our estimates of the megathrust frictional properties show that the Arauco Peninsula area has positive but relatively low (a-b)sigma(n) values (0.01 similar to 0.22MPa), that would have allowed dynamic rupture propagation into this rate-strengthening area and afterslip. Given the only modestly rate-strengthening megathrust friction in this region, the barrier effect may be attributed to its relatively large size of the rate-strengthening patch. Coseismic and postseismic uplift of the Arauco Peninsula exceeds interseismic subsidence since the time of the last major earthquake in 1835, suggesting that coseismic and postseismic deformation has resulted in some permanent strain in the forearc. C1 [Lin, Yu-nung Nina; Ortega-Culaciati, Francisco; Simons, Mark; Avouac, Jean-Philippe; Genrich, Jeff] CALTECH, Pasadena, CA 91125 USA. [Sladen, Anthony] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Geoazur, Valbonne, France. [Fielding, Eric J.] Jet Prop Lab, La Canada Flintridge, CA USA. [Brooks, Benjamin A.] Univ Hawaii, Honolulu, HI 96822 USA. [Bevis, Michael] Ohio State Univ, Columbus, OH 43210 USA. [Rietbrock, Andreas] Univ Liverpool, Liverpool L69 3BX, Merseyside, England. [Vigny, Christophe] Ecole Normale Super, F-75231 Paris, France. [Smalley, Robert] Univ Memphis, Memphis, TN 38152 USA. [Socquet, Anne] Univ Grenoble 1, Grenoble, France. RP Lin, YNN (reprint author), CALTECH, C100-23,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM ninalin@gps.caltech.edu RI Simons, Mark/N-4397-2015; Avouac, Jean-Philippe/B-5699-2015; Socquet, Anne/A-5698-2011; Fielding, Eric/A-1288-2007; Sladen, Anthony/A-2532-2017 OI Simons, Mark/0000-0003-1412-6395; Avouac, Jean-Philippe/0000-0002-3060-8442; Socquet, Anne/0000-0002-9208-7136; Fielding, Eric/0000-0002-6648-8067; Sladen, Anthony/0000-0003-4126-0020 FU NSF [EAR-1118239]; Gordon and Betty Moore Foundation [423.01]; NASA; National Aeronautics and Space Administration; CONICYT; CNRS; ANR [ANR-05-CATT-014] FX We thank Matthew Pritchard, the other reviewer and the associate editor of JGR-Solid Earth, for valuable comments and suggestions. We thank Shengji Wei at Caltech for providing the coseismic deformation model for the Pichilemu aftershock. We also thank Nadaya Cubas for her valuable discussions and help in interpreting the frictional properties. ALOS data is copyright Japanese Aerospace Exploration Agency and METI and provided through the U.S. Government Research Consortium Data Pool at the Alaska Satellite Facility and through the Group on Earth Observation Geohazards Supersite. This research is co-funded by NSF grant EAR-1118239, the Gordon and Betty Moore Foundation through Grant GBMF #423.01 to the Caltech Tectonics Observatory, and the NASA Earth Surface and Interior focus area and carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Part of the cGPS data used for this study have been acquired under the Chilean-French international collaboration "LIA Montessus de ballore," supported by CONICYT and CNRS; and ANR project SUBCHILE (grant #ANR-05-CATT-014). This paper is Caltech Tectonic Observatory contribution 211 and Seismolab contribution 10088. NR 102 TC 37 Z9 37 U1 2 U2 31 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD JUN PY 2013 VL 118 IS 6 BP 3142 EP 3159 DI 10.1002/jgrb.50207 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 295LW UT WOS:000330118600032 ER PT J AU Wang, DH Zhu, P Yin, JF Li, XF Tao, WK AF Wang, Donghai Zhu, Ping Yin, Jinfang Li, Xiaofan Tao, Wei-Kuo TI Effects of Vertical Wind Shear, Radiation, and Ice Clouds on Precipitation Distributions During a Landfall of Severe Tropical Storm, Bilis (2006) SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES LA English DT Article DE Vertical wind shear; Radiation; Ice clouds; Rainfall; Severe cloud-resolving model simulation ID MICROSCALE STRUCTURE; RAINFALL PROCESSES; FRONTAL RAINBANDS; RESOLVING MODEL; WATER; MESOSCALE; BUDGETS; HEAT; PARAMETERIZATIONS; ORGANIZATION AB Torrential rainfall responses to vertical wind shear, radiation, and ice clouds during the landfall of severe Tropical Storm, Bilis (2006) are investigated via a rainfall partitioning analysis of grid-scale sensitivity experiment data. The rainfall data are partitioned into eight types based on surface rainfall budget. The largest contributions to total rainfall come from local atmospheric moistening, water vapor convergence, and hydrometeor loss/convergence (Type 3; 29%) when the large-scale upward motions occurred only in the upper troposphere on 15 July 2006. When the large-scale upward motion center moved to the mid troposphere on 16 July, Type 3 hydrometeor loss/convergence (26%) plus local atmospheric drying, water vapor divergence, and hydrometeor loss/convergence (Type 5; 25%) show equally important contributions to total rainfall. The exclusion of vertical wind shear primarily reduced Type 5 rainfall because of the weakened hydrometeor loss/convergence on 16 July. The removal of cloud radiative effects enhances Type 5 rainfall due to increased local atmospheric drying and hydrometeor loss/convergence on 15 July. The elimination of ice clouds generally reduced Type 2 rainfall through the decreases in local atmospheric drying, water vapor convergence, and hydrometeor gain/divergence and Type 3 rainfall over two days. C1 [Wang, Donghai; Yin, Jinfang] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing, Peoples R China. [Wang, Donghai] Sci Syst & Applicat Inc, Lanham, MD USA. [Zhu, Ping] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. [Li, Xiaofan] NOAA, NESDIS, Ctr Satellite Applicat & Res, Camp Springs, MD USA. [Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, DH (reprint author), Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing, Peoples R China. EM d.wang@hotmail.com RI Li, Xiaofan/G-2094-2014 FU State Key Basic Research Development Program [2012CB417204, 2009CB421504]; Ministry of Finance; Ministry of Science and Technology [GYHY200806007, GYHY201006014, GYHY201206039]; National Natural Science Foundation [40875022, 40633016, 41175064]; State Key Laboratory of Severe Weather, Chinese Academy of Meteorological Sciences FX The authors thank Prof. B. Jou at the National Taiwan University and an anonymous reviewer for their constructive comments. This research is jointly supported by the State Key Basic Research Development Program (2012CB417204, 2009CB421504), the R&D Special Fund for Public Welfare Industry (meteorology) by the Ministry of Finance and the Ministry of Science and Technology (GYHY200806007, GYHY201006014 and GYHY201206039), the National Natural Science Foundation (40875022, 40633016, and 41175064), and the Basic Research Project of the State Key Laboratory of Severe Weather, Chinese Academy of Meteorological Sciences. NR 32 TC 0 Z9 0 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 JUN PY 2013 VL 24 IS 3 BP 383 EP 392 DI 10.3319/TAO.2013.01.11.02(A) PG 10 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Oceanography SC Geology; Meteorology & Atmospheric Sciences; Oceanography GA 292ID UT WOS:000329894500008 ER PT J AU Eckart, ME Adams, JS Bandler, SR Busch, SE Chervenak, JA Ewin, AJ Finkbeiner, FM Kelley, RL Kilbourne, CA Porter, FS Porst, JP Sadleir, JE Smith, SJ Wassell, EJ Figueroa-Feliciano, E AF Eckart, M. E. Adams, J. S. Bandler, S. R Busch, S. E. Chervenak, J. A. Ewin, A. J. Finkbeiner, F. M. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Porst, J.-P. Sadleir, J. E. Smith, S. J. Wassell, E. J. Figueroa-Feliciano, E. TI Development of TES Microcalorimeter Arrays for the Micro-X Sounding Rocket Experiment SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Astrophysics; superconducting devices; X-ray detectors AB The Micro-X sounding rocket program will fly a 128-pixel array of transition-edge-sensor microcalorimeters to enable high-resolution X-ray imaging spectroscopy of supernova remnants. To match the angular resolution of the optics while maximizing the field-of-view and retaining a high energy resolution (2-4 eV at 1 keV), we have designed the pixels using 590 x 590 mu m(2) Au/Bi absorbers, which overhang 140 x 140 mu m(2) Mo/Au sensors. Here we report experimental results from flight-candidate arrays, including measurements of energy resolution, uniformity, and absorber thermalization. We describe the reduction in pixel-to-pixel crosstalk afforded by an angle-evaporated Cu backside heatsinking layer, which provides Cu coverage on the four sidewalls of the silicon wells beneath each pixel. In addition, we present measurements of devices that have an identical pixel architecture but were fabricated with thin (sub-micron) all-Au absorbers. C1 [Eckart, M. E.; Adams, J. S.; Bandler, S. R; Busch, S. E.; Chervenak, J. A.; Ewin, A. J.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Porst, J.-P.; Sadleir, J. E.; Smith, S. J.; Wassell, E. J.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eckart, M. E.; Adams, J. S.; Bandler, S. R; Smith, S. J.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Finkbeiner, F. M.] Wyle Informat Syst, McLean, VA 22102 USA. [Porst, J.-P.] Brown Univ, Providence, RI 02912 USA. [Wassell, E. J.] MEI Technol Inc, Seabrook, MD 20706 USA. [Figueroa-Feliciano, E.] MIT, Cambridge, MA 02139 USA. RP Eckart, ME (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Megan.E.Eckart@nasa.gov RI Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119 FU NASA Postdoctoral Program at GSFC; ORAU FX S. E. Busch was supported in part by an appointment to the NASA Postdoctoral Program at GSFC, administered by ORAU through a contract with NASA. NR 13 TC 1 Z9 1 U1 0 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2101705 DI 10.1109/TASC.2013.2244631 PN 1 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100081 ER PT J AU Bednarcyk, BA Yarrington, PW Arnold, SM AF Bednarcyk, Brett A. Yarrington, Phillip W. Arnold, Steven M. TI Multiscale Fatigue Life Prediction for Composite Panels SO CMC-COMPUTERS MATERIALS & CONTINUA LA English DT Article ID HONEYCOMB SANDWICH BEAMS; STRENGTH; FOAM; CELLS AB Fatigue life prediction capabilities have been incorporated into the HyperSizer Composite Analysis and Structural Sizing Software. The fatigue damage model is introduced at the fiber/matrix constituent scale through HyperSizer's coupling with NASA's MAC/GMC micromechanics software. This enables prediction of the micro scale damage progression throughout stiffened and sandwich panels as a function of cycles leading ultimately to simulated panel failure. The fatigue model implementation uses a cycle jumping technique such that, rather than applying a specified number of additional cycles, a specified local damage increment is specified and the number of additional cycles to reach this damage increment is calculated. In this way, the effect of stress redistribution due to damage-induced stiffness change is captured, but the fatigue simulations remain computationally efficient. The model is compared to experimental fatigue life data for two composite facesheet/foam core sandwich panels, demonstrating very good agreement. C1 [Bednarcyk, Brett A.; Arnold, Steven M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Yarrington, Phillip W.] Collier Res Corp, Newport News, VA 23606 USA. RP Bednarcyk, BA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. FU NASA's Aviation Safety Program Integrated Vehicle Health Management Project [NNC07CN66C] FX The second author gratefully acknowledges funding for this work provided by NASA's Aviation Safety Program Integrated Vehicle Health Management Project (Contract NNC07CN66C) with Dr. Steven M. Arnold as Technical Monitor. In addition, the authors acknowledge several helpful communications with Dan Zenkert of Kungliga Tekniska Hogskolan, Stockholm, Sweden, regarding the experimental data presented herein. NR 31 TC 0 Z9 0 U1 1 U2 5 PU TECH SCIENCE PRESS PI NORCROSS PA 6825 JIMMY CARTER BLVD, STE 1850, NORCROSS, GA 30071 USA SN 1546-2218 EI 1546-2226 J9 CMC-COMPUT MATER CON JI CMC-Comput. Mat. Contin. PD JUN PY 2013 VL 35 IS 3 BP 229 EP 254 PG 26 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary; Mathematics, Interdisciplinary Applications SC Engineering; Materials Science; Mathematics GA 255GJ UT WOS:000327227100003 ER PT J AU Hodges, J AF Hodges, Jan TI The Mutiny at Pisgah Forest SO PROLOGUE-QUARTERLY OF THE NATIONAL ARCHIVES AND RECORDS ADMINISTRATION LA English DT Article C1 [Hodges, Jan] Natl Archives, College Pk, MD USA. [Hodges, Jan] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Hodges, J (reprint author), Natl Archives, College Pk, MD USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ARCHIVES RECORDS ADMINISTRATION PI WASHINGTON PA TRUST FUND BOARD, WASHINGTON, DC 20408 USA SN 0033-1031 J9 PROLOGUE JI Prologue PD SUM PY 2013 VL 45 IS 2 BP 28 EP 35 PG 8 WC History SC History GA 257BS UT WOS:000327358900006 ER PT J AU Blossey, PN Bretherton, CS Zhang, MH Cheng, AN Endo, S Heus, T Liu, YG Lock, AP de Roode, SR Xu, KM AF Blossey, Peter N. Bretherton, Christopher S. Zhang, Minghua Cheng, Anning Endo, Satoshi Heus, Thijs Liu, Yangang Lock, Adrian P. de Roode, Stephan R. Xu, Kuan-Man TI Marine low cloud sensitivity to an idealized climate change: The CGILS LES intercomparison SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article DE cloud feedbacks ID LARGE-EDDY SIMULATION; BOUNDARY-LAYER CLOUDS; STRATIFORM CLOUDS; STRATOCUMULUS; MODEL; PARAMETERIZATION; FEEDBACKS; UNCERTAINTIES; ENTRAINMENT; FORMULATION AB Subtropical marine low cloud sensitivity to an idealized climate change is compared in six large-eddy simulation (LES) models as part of CGILS. July cloud cover is simulated at three locations over the subtropical northeast Pacific Ocean, which are typified by cold sea surface temperatures (SSTs) under well-mixed stratocumulus, cool SSTs under decoupled stratocumulus, and shallow cumulus clouds overlying warmer SSTs. The idealized climate change includes a uniform 2 K SST increase with corresponding moist-adiabatic warming aloft and subsidence changes, but no change in free-tropospheric relative humidity, surface wind speed, or CO2. For each case, realistic advective forcings and boundary conditions are generated for the control and perturbed states which each LES runs for 10 days into a quasi-steady state. For the control climate, the LESs correctly produce the expected cloud type at all three locations. With the perturbed forcings, all models simulate boundary-layer deepening due to reduced subsidence in the warmer climate, with less deepening at the warm-SST location due to regulation by precipitation. The models do not show a consistent response of liquid water path and albedo in the perturbed climate, though the majority predict cloud thickening (negative cloud feedback) at the cold-SST location and slight cloud thinning (positive cloud feedback) at the cool-SST and warm-SST locations. In perturbed climate simulations at the cold-SST location without the subsidence decrease, cloud albedo consistently decreases across the models. Thus, boundary-layer cloud feedback on climate change involves compensating thermodynamic and dynamic effects of warming and may interact with patterns of subsidence change. C1 [Blossey, Peter N.; Bretherton, Christopher S.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Zhang, Minghua] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Cheng, Anning] Sci Syst & Applicat Inc, Hampton, VA USA. [Endo, Satoshi; Liu, Yangang] Brookhaven Natl Lab, Div Atmospher Sci, Upton, NY 11973 USA. [Heus, Thijs] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Lock, Adrian P.] Met Off, Fdn Sci, Exeter, Devon, England. [de Roode, Stephan R.] Delft Univ Technol, Dept Multiscale Phys, Delft, Netherlands. [Xu, Kuan-Man] NASA Langley Res Ctr, Sci Directorate, Hampton, VA USA. RP Blossey, PN (reprint author), Univ Washington, Box 351640, Seattle, WA 98195 USA. EM pblossey@uw.edu RI Liu, Yangang/H-6154-2011; Xu, Kuan-Man/B-7557-2013; Heus, Thijs/E-7336-2012 OI Xu, Kuan-Man/0000-0001-7851-2629; Heus, Thijs/0000-0003-2650-2423 FU Center for Multiscale Modeling and Prediction (CMMAP); NSF; European Union Cloud Intercomparison, Process Study & Evaluation Project (EUCLIPSE); European Union; Deutscher Wetter Dienst (DWD) through the Hans-Ertel Centre for Weather Research; National Computing Facilities Foundation (NCF); U.S. Department of Energy (DOE) Earth System Modeling (ESM) program through the FASTER project; NASA Modeling and Analysis Program (MAP); U.S. National Science Foundation FX Blossey and Bretherton acknowledge support from the Center for Multiscale Modeling and Prediction (CMMAP), supported by NSF. The authors also thank Marat Khairoutdinov of Stony Brook University for his sustained leadership in maintaining SAM, Matthew Wyant for providing Figure 5, and Andy Ackerman for proposing the approach for computing effective radius. De Roode is supported through the European Union Cloud Intercomparison, Process Study & Evaluation Project (EUCLIPSE), funded under Framework Program 7 of the European Union. Heus was funded by the Deutscher Wetter Dienst (DWD) through the Hans-Ertel Centre for Weather Research. The simulations with the Dutch LES model were sponsored by the National Computing Facilities Foundation (NCF). Endo, Liu, and Zhang were supported by the U.S. Department of Energy (DOE) Earth System Modeling (ESM) program through the FASTER project (www.bnl.gov/esm). Zhang was also supported by the NASA Modeling and Analysis Program (MAP) and the U.S. National Science Foundation. The authors would also like to thank two anonymous referees for their comments. NR 53 TC 43 Z9 43 U1 2 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD JUN PY 2013 VL 5 IS 2 BP 234 EP 258 DI 10.1002/jame.20025 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229OR UT WOS:000325277300015 ER PT J AU An, D Ramirez, SV Sellgren, K AF An, Deokkeun Ramirez, Solange V. Sellgren, Kris TI THE GALACTIC CENTER: NOT AN ACTIVE GALACTIC NUCLEUS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: ISM; galaxies: nuclei; galaxies: starburst; infrared: ISM ISM: molecules; stars: formation ID CENTER MOLECULAR CLOUDS; CENTER INTERSTELLAR-MEDIUM; SPITZER-SPACE-TELESCOPE; NEARBY GALAXIES SURVEY; YOUNG STELLAR OBJECTS; CENTER REGION; X-RAYS; SPECTROSCOPIC IDENTIFICATION; CHEMICAL ABUNDANCES; STARBURST GALAXIES AB We present 10 mu m-35 mu m Spitzer spectra of the interstellar medium in the Central Molecular Zone (CMZ), the central 210 pc x 60 pc of the Galactic center (GC). We present maps of the CMZ in ionic and H2 emission, covering a more extensive area than earlier spectroscopic surveys in this region. The radial velocities and intensities of ionic lines and H2 suggest that most of the H-2 0-0 S(0) emission comes from gas along the line-of-sight, as found by previous work. We compare diagnostic line ratios measured in the Spitzer Infrared Nearby Galaxies Survey to our data. Previous work shows that forbidden line ratios can distinguish star-forming galaxies from low-ionization nuclear emission-line regions (LINERs) and active galactic nuclei (AGNs). Our GC line ratios agree with star-forming galaxies and not with LINERs or AGNs. C1 [An, Deokkeun] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea. [Ramirez, Solange V.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Sellgren, Kris] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP An, D (reprint author), Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea. EM deokkeun@ewha.ac.kr NR 60 TC 2 Z9 2 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2013 VL 206 IS 2 AR UNSP 20 DI 10.1088/0067-0049/206/2/20 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 234OX UT WOS:000325654800011 ER PT J AU Galametz, A Grazian, A Fontana, A Ferguson, HC Ashby, MLN Barro, G Castellano, M Dahlen, T Donley, JL Faber, SM Grogin, N Guo, Y Huang, KH Kocevski, DD Koekemoer, AM Lee, KS McGrath, EJ Peth, M Willner, SP Almaini, O Cooper, M Cooray, A Conselice, CJ Dickinson, M Dunlop, JS Fazio, GG Foucaud, S Gardner, JP Giavalisco, M Hathi, NP Hartley, WG Koo, DC Lai, K de Mello, DF McLure, RJ Lucas, RA Paris, D Pentericci, L Santini, P Simpson, C Sommariva, V Targett, T Weiner, BJ Wuyts, S AF Galametz, Audrey Grazian, Andrea Fontana, Adriano Ferguson, Henry C. Ashby, M. L. N. Barro, Guillermo Castellano, Marco Dahlen, Tomas Donley, Jennifer L. Faber, Sandy M. Grogin, Norman Guo, Yicheng Huang, Kuang-Han Kocevski, Dale D. Koekemoer, Anton M. Lee, Kyoung-Soo McGrath, Elizabeth J. Peth, Michael Willner, S. P. Almaini, Omar Cooper, Michael Cooray, Asantha Conselice, Christopher J. Dickinson, Mark Dunlop, James S. Fazio, G. G. Foucaud, Sebastien Gardner, Jonathan P. Giavalisco, Mauro Hathi, N. P. Hartley, Will G. Koo, David C. Lai, Kamson de Mello, Duilia F. McLure, Ross J. Lucas, Ray A. Paris, Diego Pentericci, Laura Santini, Paola Simpson, Chris Sommariva, Veronica Targett, Thomas Weiner, Benjamin J. Wuyts, Stijn CA CANDELS Team TI CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: photometry; methods: data analysis; techniques: image processing ID EXTRAGALACTIC LEGACY SURVEY; GALAXY LUMINOSITY FUNCTION; SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; EARLY DATA RELEASE; IMAGE SUBTRACTION; EVOLUTION SURVEY; SURVEY SXDS; SELECTION; CLUSTER AB We present the multiwavelength-ultraviolet to mid-infrared-catalog of the UKIRT Infrared Deep Sky Survey (UKIDSS) Ultra-Deep Survey field observed as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). Based on publicly available data, the catalog includes the CANDELS data from the Hubble Space Telescope (near-infrared WFC3 F125W and F160W data and visible ACS F606W and F814W data); u-band data from CFHT/Megacam; B, V, R-c, i', and z' band data from Subaru/Suprime-Cam; Y and K-s band data from VLT/HAWK-I; J, H, and K band data from UKIDSS (Data Release 8); and Spitzer/IRAC data (3.6, 4.5 mu m from SEDS; 5.8 and 8.0 mu m from SpUDS). The present catalog is F160W-selected and contains 35, 932 sources over an area of 201.7 arcmin(2) and includes radio-and X-ray-detected sources and spectroscopic redshifts available for 210 sources. C1 [Galametz, Audrey; Grazian, Andrea; Fontana, Adriano; Castellano, Marco; Paris, Diego; Pentericci, Laura; Santini, Paola; Sommariva, Veronica] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Ferguson, Henry C.; Dahlen, Tomas; Grogin, Norman; Huang, Kuang-Han; Koekemoer, Anton M.; Lai, Kamson; Lucas, Ray A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ashby, M. L. N.; Willner, S. P.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barro, Guillermo; Faber, Sandy M.; Guo, Yicheng; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Donley, Jennifer L.] Los Alamos Natl Lab, Los Alamos, NM USA. [Guo, Yicheng; Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Huang, Kuang-Han; Peth, Michael] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [Almaini, Omar; Conselice, Christopher J.; Hartley, Will G.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Cooper, Michael; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA. [Dickinson, Mark] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Dunlop, James S.; McLure, Ross J.; Targett, Thomas] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh, Midlothian, Scotland. [Foucaud, Sebastien] Natl Taiwan Normal Univ, Taipei, Taiwan. [Gardner, Jonathan P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Hathi, N. P.] Observ Carnegie Inst Sci, Pasadena, CA USA. [de Mello, Duilia F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Simpson, Chris] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead, Merseyside, England. [Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Galametz, A (reprint author), INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. EM audrey.galametz@oa-roma.inaf.it RI Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Castellano, Marco/0000-0001-9875-8263; Weiner, Benjamin/0000-0001-6065-7483; Santini, Paola/0000-0002-9334-8705; Koekemoer, Anton/0000-0002-6610-2048; fontana, adriano/0000-0003-3820-2823 NR 54 TC 73 Z9 73 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2013 VL 206 IS 2 AR UNSP 10 DI 10.1088/0067-0049/206/2/10 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 234OX UT WOS:000325654800001 ER PT J AU Seader, S Tenenbaum, P Jenkins, JM Burke, CJ AF Seader, Shawn Tenenbaum, Peter Jenkins, Jon M. Burke, Christopher J. TI chi(2) DISCRIMINATORS FOR TRANSITING PLANET DETECTION IN KEPLER DATA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE methods: statistical ID ERROR-CORRECTION; LIGHT CURVES; SCIENCE AB The Kepler spacecraft observes a host of target stars to detect transiting planets. Requiring a 7.1s detection in three years of data yields over 100,000 detections, many of which are false alarms. After a second cut is made on a robust detection statistic, some 50,000 or more targets still remain. These false alarms waste resources as they propagate through the remainder of the software pipeline and so a method to discriminate against them is crucial in maintaining the desired sensitivity to true events. This paper describes a.2 test which represents a novel application of an existing formalism developed for false alarm mitigation in searches for gravitational waves. Using this technique, the false alarm rate can be lowered to similar to 5%. C1 [Seader, Shawn; Tenenbaum, Peter; Jenkins, Jon M.; Burke, Christopher J.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Seader, S (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. EM shawn.seader@nasa.gov; peter.tenenbaum@nasa.gov; jon.jenkins@nasa.gov; christopher.j.burke@nasa.gov FU NASA's Science Mission Directorate FX The author thanks Bruce Allen for the original work on this subject on whichmost of this work is based. Kepler was selected as the 10th mission of NASA's Discovery Program. Funding for this work is provided by NASA's Science Mission Directorate. NR 18 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2013 VL 206 IS 2 AR UNSP 25 DI 10.1088/0067-0049/206/2/25 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 234OX UT WOS:000325654800016 ER PT J AU Adrian-Martinez, S Al Samarai, I Albert, A Andre, M Anghinolfi, M Anton, G Anvar, S Ardid, M Astraatmadja, T Aubert, JJ Baret, B Basa, S Bertin, V Biagi, S Bigongiari, C Bogazzi, C Bou-Cabo, M Bouhou, B Bouwhuis, MC Brunner, J Busto, J Capone, A Arloganu, CC Carr, J Cecchini, S Charif, Z Charvis, P Chiarusi, T Circella, M Coniglione, R Core, L Costantini, H Coyle, P Creusot, A Curtil, C De Bonis, G Decowski, MP Dekeyser, I Deschamps, A Distefano, C Donzaud, C Dornic, D Dorosti, Q Drouhin, D Eberl, T Emanuele, U Enzenhofer, A Ernenwein, JP Escoffier, S Fehn, K Fermani, P Ferri, M Ferry, S Flaminio, V Folger, F Fritsch, U Fuda, JL Galata, S Gay, P Geyer, K Giacomelli, G Giordano, V Gomez-Gonzalez, JP Graf, K Guillard, G Hallewell, G Hamal, M van Haren, H Heijboer, AJ Hello, Y Hernandez-Rey, JJ Herold, B Hossl, J Hsu, CC de Jong, M Kadler, M Kalekin, O Kappes, A Katz, U Kavatsyuk, O Kooijman, P Kopper, C Kouchner, A Kreykenbohm, I Kulikovskiy, V Lahmann, R Lambard, G Larosa, G Lattuada, D Lefevre, D Lim, G Lo Presti, D Loehner, H Loucatos, S Louis, F Mangano, S Marcelin, M Margiotta, A Martinez-Mora, JA Martini, S Meli, A Montaruli, T Morganti, M Moscoso, L Motz, H Neff, M Nezri, E Palioselitis, D Pavalas, GE Payet, K Petrovic, J Piattelli, P Popa, V Pradier, T Presani, E Racca, C Reed, C Riccobene, G Richardt, C Richter, R Riviere, C Robert, A Roensch, K Rostovtsev, A Ruiz-Rivas, J Rujoiu, M Russo, GV Samtleben, DFE Sanchez-Losa, A Sapienza, P Schmid, J Schnabel, J Schock, F Schuller, JP Schussler, F Seitz, T Shanidze, R Simeone, F Spies, A Spurio, M Steijger, JJM Stolarczyk, T Taiuti, M Tamburini, C Trovato, A Vallage, B Vallee, C Van Elewyck, V Vecchi, M Vernin, P Visser, E Wagner, S Wijnker, G Wilms, J de Wolf, E Yepes, H Zaborov, D Zornoza, JD Zuniga, J Aasi, J Abadie, J Abbott, BP Abbott, R Abbott, TD Abernathy, M Accadia, T Acernese, F Adams, C Adams, T Addesso, P Adhikari, R Affeldt, C Agathos, M Agatsuma, K Ajith, P Allen, B Allocca, A Ceron, EA Amariutei, D Anderson, SB Anderson, WG Arai, K Araya, MC Ast, S Aston, SM Astone, P Atkinson, D Aufmuth, P Aulbert, C Aylott, BE Babak, S Baker, P Ballardin, G Ballmer, S Bao, Y Barayoga, JCB Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Bastarrika, M Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Beck, D Behnke, B Bejger, M Beker, MG Bell, AS Bell, C Belopolski, I Benacquista, M Berliner, JM Bertolini, A Betzwieser, J Beveridge, N Beyersdorf, PT Bhadbade, T Bilenko, IA Billingsley, G Birch, J Biswas, R Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Bland, B Blom, M Bock, O Bodiya, TP Bogan, C Bond, C Bondarescu, R Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Braccini, S Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Bulik, T Bulten, HJ Buonanno, A Burguet-Castell, J Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Calloni, E Camp, JB Campsie, P Cannon, K Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chalermsongsak, T Charlton, P Chassande-Mottin, E Chen, W Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chua, SSY Chung, CTY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Clayton, JH Cleva, F Coccia, E Cohadon, PF Colacino, CN Colla, A Colombini, M Conte, A Conte, R Cook, D Corbitt, TR Cordier, M Cornish, N Corsi, A Costa, CA Coughlin, M Coulon, JP Couvares, P Coward, DM Cowart, M Coyne, DC Creighton, JDE Creighton, TD Cruise, AM Cumming, A Cunningham, L Cuoco, E Cutler, RM Dahl, K Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daudert, B Daveloza, H Davier, M Daw, EJ Day, R Dayanga, T De Rosa, R Debra, D Debreczeni, G Degallaix, J Del Pozzo, W Dent, T Dergachev, V DeRosa, R Dhurandhar, S Di Fiore, L Di Lieto, A Di Palma, I Emilio, MD Di Virgilio, A Diaz, M Dietz, A Donovan, F Dooley, KL Doravari, S Dorsher, S Drago, M Drever, RWP Driggers, JC Du, Z Dumas, JC Dwyer, S Eberle, T Edgar, M Edwards, M Effler, A Ehrens, P Endroczi, G Engel, R Etzel, T Evans, K Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Farr, BF Favata, M Fazi, D Fehrmann, H Feldbaum, D Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, RP Flaminio, R Foley, S Forsi, E Forte, LA Fotopoulos, N Fournier, JD Franc, J Franco, S Frasca, S Frasconi, F Frede, M Frei, MA Frei, Z Freise, A Frey, R Fricke, TT Friedrich, D Fritschel, P Frolov, VV Fujimoto, MK Fulda, PJ Fyffe, M Gair, J Galimberti, M Gammaitoni, L Garcia, J Garufi, F Gaspar, ME Gelencser, G Gemme, G Genin, E Gennai, A Gergely, LA Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gil-Casanova, S Gill, C Gleason, J Goetz, E Gonzalez, G Gorodetsky, ML Gossler, S Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gray, C Greenhalgh, RJS Gretarsson, AM Griffo, C Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gupta, R Gustafson, EK Gustafson, R Hallam, JM Hammer, D Hammond, G Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hartman, MT Haughian, K Hayama, K Hayau, JF Heefner, J Heidmann, A Heintze, MC Heitmann, H Hello, P Hemming, G Hendry, MA Heng, IS Heptonstall, AW Herrera, V Heurs, M Hewitson, M Hild, S Hoak, D Hodge, KA Holt, K Holtrop, M Hong, T Hooper, S Hough, J Howell, EJ Hughey, B Husa, S Huttner, SH Huynh-Dinh, T Ingram, DR Inta, R Isogai, T Ivanov, A Izumi, K Jacobson, M James, E Jang, YJ Jaranowski, P Jesse, E Johnson, WW Jones, DI Jones, R Jonker, RJG Ju, L Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kasprzack, M Kasturi, R Katsavounidis, E Katzman, W Kaufer, H Kaufman, K Kawabe, K Kawamura, S Kawazoe, F Keitel, D Kelley, D Kells, W Keppel, DG Keresztes, Z Khalaidovski, A Khalili, FY Khazanov, EA Kim, BK Kim, C Kim, H Kim, K Kim, N Kim, YM King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, D Kringel, V Krishnan, B Krolak, A Kuehn, G Kumar, P Kumar, R Kurdyumov, R Kwee, P Lam, PK Landry, M Langley, A Lantz, B Lastzka, N Lawrie, C Lazzarini, A Le Roux, A Leaci, P Lee, CH Lee, HK Lee, HM Leong, JR Leonor, I Leroy, N Letendre, N Lhuillier, V Li, J Li, TGF Lindquist, PE Litvine, V Liu, Y Liu, Z Lockerbie, NA Lodhia, D Logue, J Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Lubinski, M Lueck, H Lundgren, AP Macarthur, J Macdonald, E Machenschalk, B MacInnis, M Macleod, DM Mageswaran, M Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Mandel, I Mandic, V Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J Martelli, F Martin, IW Martin, RM Marx, JN Mason, K Masserot, A Matichard, F Matone, L Matzner, RA Mavalvala, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIver, J Meadors, GD Mehmet, M Meier, T Melatos, A Melissinos, AC Mendell, G Menendez, DF Mercer, RA Meshkov, S Messenger, C Meyer, MS Miao, H Michel, C Milano, L Miller, J Minenkov, Y Mingarelli, CMF Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Mohan, M Mohapatra, SRP Moraru, D Moreno, G Morgado, N Morgia, A Mori, T Morriss, SR Mosca, S Mossavi, K Mours, B Mow-Lowry, CM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Muller-Ebhardt, H Munch, J Murphy, D Murray, PG Mytidis, A Nash, T Naticchioni, L Necula, V Nelson, J Neri, I Newton, G Nguyen, T Nishizawa, A Nitz, A Nocera, F Nolting, D Normandin, ME Nuttall, L Ochsner, E O'Dell, J Oelker, E Ogin, GH Oh, JJ Oh, SH Oldenberg, RG O'Reilly, B O'Shaughnessy, R Osthelder, C Ott, CD Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Page, A Palladino, L Palomba, C Pan, Y Pankow, C Paoletti, F Paoletti, R Papa, MA Parisi, M Pasqualetti, A Passaquieti, R Passuello, D Pedraza, M Penn, S Perreca, A Persichetti, G Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pierro, V Pihlaja, M Pinard, L Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Poggiani, R Pold, J Postiglione, F Poux, C Prato, M Predoi, V Prestegard, T Price, LR Prijatelj, M Principe, M Privitera, S Prix, R Prodi, GA Prokhorov, LG Puncken, O Punturo, M Puppo, P Quetschke, V Quitzow-James, R Raab, FJ Rabeling, DS Racz, I Radkins, H Raffai, P Rakhmanov, M Ramet, C Rankins, B Rapagnani, P Raymond, V Re, V Reed, CM Reed, T Regimbau, T Reid, S Reitze, DH Ricci, F Riesen, R Riles, K Roberts, M Robertson, NA Robinet, F Robinson, C Robinson, EL Rocchi, A Roddy, S Rodriguez, C Rodruck, M Rolland, L Rollins, JG Romano, JD Romano, R Romie, JH Rosinska, D Rover, C Rowan, S Rudiger, A Ruggi, P Ryan, K Salemi, F Sammut, L Sandberg, V Sankar, S Sannibale, V Santamaria, L Santiago-Prieto, I Santostasi, G Saracco, E Sassolas, B Sathyaprakash, BS Saulson, PR Savage, RL Schilling, R Schnabel, R Schofield, RMS Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Seifert, F Sellers, D Sentenac, D Sergeev, A Shaddock, DA Shaltev, M Shapiro, B Shawhan, P Shoemaker, DH Sidery, TL Siemens, X Sigg, D Simakov, D Singer, A Singer, L Sintes, AM Skelton, GR Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, RJE Smith-Lefebvre, ND Somiya, K Sorazu, B Speirits, FC Sperandio, L Stefszky, M Steinert, E Steinlechner, J Steinlechner, S Steplewski, S Stochino, A Stone, R Strain, KA Strigin, SE Stroeer, AS Sturani, R Stuver, AL Summerscales, TZ Sung, M Susmithan, S Sutton, PJ Swinkels, B Szeifert, G Tacca, M Taffarello, L Talukder, D Tanner, DB Tarabrin, SP Taylor, R ter Braack, APM Thomas, P Thorne, KA Thorne, KS Thrane, E Thuring, A Titsler, C Tokmakov, KV Tomlinson, C Toncelli, A Tonelli, M Torre, O Torres, CV Torrie, CI Tournefier, E Travasso, F Traylor, G Tse, M Ugolini, D Vahlbruch, H Vajente, G van den Brand, JFJ Van den Broeck, C van der Putten, S van Veggel, AA Vass, S Vasuth, M Vaulin, R Vavoulidis, M Vecchio, A Vedovato, G Veitch, J Veitch, PJ Venkateswara, K Verkindt, D Vetrano, F Vicere, A Villar, AE Vinet, JY Vitale, S Vocca, H Vorvick, C Vyatchanin, SP Wade, A Wade, L Wade, M Waldman, SJ Wallace, L Wan, Y Wang, M Wang, X Wanner, A Ward, RL Was, M Weinert, M Weinstein, AJ Weiss, R Welborn, T Wen, L Wessels, P West, M Westphal, T Wette, K Whelan, JT Whitcomb, SE White, DJ Whiting, BF Wiesner, K Wilkinson, C Willems, PA Williams, L Williams, R Willke, B Wimmer, M Winkelmann, L Winkler, W Wipf, CC Wiseman, AG Wittel, H Woan, G Wooley, R Worden, J Yablon, J Yakushin, I Yamamoto, H Yamamoto, K Yancey, CC Yang, H Yeaton-Massey, D Yoshida, S Yvert, M Zadrozny, A Zanolin, M Zendri, JP Zhang, F Zhang, L Zhao, C Zotov, N Zucker, ME Zweizig, J AF Adrian-Martinez, S. Al Samarai, I. Albert, A. Andre, M. Anghinolfi, M. Anton, G. Anvar, S. Ardid, M. Astraatmadja, T. Aubert, J-J. Baret, B. Basa, S. Bertin, V. Biagi, S. Bigongiari, C. Bogazzi, C. Bou-Cabo, M. Bouhou, B. Bouwhuis, M. C. Brunner, J. Busto, J. Capone, A. Arloganu, C. C. Carr, J. Cecchini, S. Charif, Z. Charvis, Ph. Chiarusi, T. Circella, M. Coniglione, R. Core, L. Costantini, H. Coyle, P. Creusot, A. Curtil, C. De Bonis, G. Decowski, M. P. Dekeyser, I. Deschamps, A. Distefano, C. Donzaud, C. Dornic, D. Dorosti, Q. Drouhin, D. Eberl, T. Emanuele, U. Enzenhoefer, A. Ernenwein, J-P. Escoffier, S. Fehn, K. Fermani, P. Ferri, M. Ferry, S. Flaminio, V. Folger, F. Fritsch, U. Fuda, J-L. Galata, S. Gay, P. Geyer, K. Giacomelli, G. Giordano, V. Gomez-Gonzalez, J. P. Graf, K. Guillard, G. Hallewell, G. Hamal, M. van Haren, H. Heijboer, A. J. Hello, Y. Hernandez-Rey, J. J. Herold, B. Hoessl, J. Hsu, C. C. de Jong, M. Kadler, M. Kalekin, O. Kappes, A. Katz, U. Kavatsyuk, O. Kooijman, P. Kopper, C. Kouchner, A. Kreykenbohm, I. Kulikovskiy, V. Lahmann, R. Lambard, G. Larosa, G. Lattuada, D. Lefevre, D. Lim, G. Lo Presti, D. Loehner, H. Loucatos, S. Louis, F. Mangano, S. Marcelin, M. Margiotta, A. Martinez-Mora, J. A. Martini, S. Meli, A. Montaruli, T. Morganti, M. Moscoso, L. Motz, H. Neff, M. Nezri, E. Palioselitis, D. Pavalas, G. E. Payet, K. Petrovic, J. Piattelli, P. Popa, V. Pradier, T. Presani, E. Racca, C. Reed, C. Riccobene, G. Richardt, C. Richter, R. Riviere, C. Robert, A. Roensch, K. Rostovtsev, A. Ruiz-Rivas, J. Rujoiu, M. Russo, G. V. Samtleben, D. F. E. Sanchez-Losa, A. Sapienza, P. Schmid, J. Schnabel, J. Schoeck, F. Schuller, J-P. Schuessler, F. Seitz, T. Shanidze, R. Simeone, F. Spies, A. Spurio, M. Steijger, J. J. M. Stolarczyk, Th. Taiuti, M. Tamburini, C. Trovato, A. Vallage, B. Vallee, C. Van Elewyck, V. Vecchi, M. Vernin, P. Visser, E. Wagner, S. Wijnker, G. Wilms, J. de Wolf, E. Yepes, H. Zaborov, D. Zornoza, J. D. Zuniga, J. Aasi, J. Abadie, J. Abbott, B. P. Abbott, R. Abbott, T. D. Abernathy, M. Accadia, T. Acernese, F. Adams, C. Adams, T. Addesso, P. Adhikari, R. Affeldt, C. Agathos, M. Agatsuma, K. Ajith, P. Allen, B. Allocca, A. Ceron, E. Amador Amariutei, D. Anderson, S. B. Anderson, W. G. Arai, K. Araya, M. C. Ast, S. Aston, S. M. Astone, P. Atkinson, D. Aufmuth, P. Aulbert, C. Aylott, B. E. Babak, S. Baker, P. Ballardin, G. Ballmer, S. Bao, Y. Barayoga, J. C. B. Barker, D. Barone, F. Barr, B. Barsotti, L. Barsuglia, M. Barton, M. A. Bartos, I. Bassiri, R. Bastarrika, M. Basti, A. Batch, J. Bauchrowitz, J. Bauer, Th. S. Bebronne, M. Beck, D. Behnke, B. Bejger, M. Beker, M. G. Bell, A. S. Bell, C. Belopolski, I. Benacquista, M. Berliner, J. M. Bertolini, A. Betzwieser, J. Beveridge, N. Beyersdorf, P. T. Bhadbade, T. Bilenko, I. A. Billingsley, G. Birch, J. Biswas, R. Bitossi, M. Bizouard, M. A. Black, E. Blackburn, J. K. Blackburn, L. Blair, D. Bland, B. Blom, M. Bock, O. Bodiya, T. P. Bogan, C. Bond, C. Bondarescu, R. Bondu, F. Bonelli, L. Bonnand, R. Bork, R. Born, M. Boschi, V. Bose, S. Bosi, L. Braccini, S. Bradaschia, C. Brady, P. R. Braginsky, V. B. Branchesi, M. Brau, J. E. Breyer, J. Briant, T. Bridges, D. O. Brillet, A. Brinkmann, M. Brisson, V. Britzger, M. Brooks, A. F. Brown, D. A. Bulik, T. Bulten, H. J. Buonanno, A. Burguet-Castell, J. Buskulic, D. Buy, C. Byer, R. L. Cadonati, L. Cagnoli, G. Calloni, E. Camp, J. B. Campsie, P. Cannon, K. Canuel, B. Cao, J. Capano, C. D. Carbognani, F. Carbone, L. Caride, S. Caudill, S. Cavaglia, M. Cavalier, F. Cavalieri, R. Cella, G. Cepeda, C. Cesarini, E. Chalermsongsak, T. Charlton, P. Chassande-Mottin, E. Chen, W. Chen, X. Chen, Y. Chincarini, A. Chiummo, A. Cho, H. S. Chow, J. Christensen, N. Chua, S. S. Y. Chung, C. T. Y. Chung, S. Ciani, G. Clara, F. Clark, D. E. Clark, J. A. Clayton, J. H. Cleva, F. Coccia, E. Cohadon, P. -F. Colacino, C. N. Colla, A. Colombini, M. Conte, A. Conte, R. Cook, D. Corbitt, T. R. Cordier, M. Cornish, N. Corsi, A. Costa, C. A. Coughlin, M. Coulon, J. -P. Couvares, P. Coward, D. M. Cowart, M. Coyne, D. C. Creighton, J. D. E. Creighton, T. D. Cruise, A. M. Cumming, A. Cunningham, L. Cuoco, E. Cutler, R. M. Dahl, K. Damjanic, M. Danilishin, S. L. D'Antonio, S. Danzmann, K. Dattilo, V. Daudert, B. Daveloza, H. Davier, M. Daw, E. J. Day, R. Dayanga, T. De Rosa, R. Debra, D. Debreczeni, G. Degallaix, J. Del Pozzo, W. Dent, T. Dergachev, V. DeRosa, R. Dhurandhar, S. Di Fiore, L. Di Lieto, A. Di Palma, I. Emilio, M. Di Paolo Di Virgilio, A. Diaz, M. Dietz, A. Donovan, F. Dooley, K. L. Doravari, S. Dorsher, S. Drago, M. Drever, R. W. P. Driggers, J. C. Du, Z. Dumas, J. -C. Dwyer, S. Eberle, T. Edgar, M. Edwards, M. Effler, A. Ehrens, P. Endroczi, G. Engel, R. Etzel, T. Evans, K. Evans, M. Evans, T. Factourovich, M. Fafone, V. Fairhurst, S. Farr, B. F. Favata, M. Fazi, D. Fehrmann, H. Feldbaum, D. Ferrante, I. Ferrini, F. Fidecaro, F. Finn, L. S. Fiori, I. Fisher, R. P. Flaminio, R. Foley, S. Forsi, E. Forte, L. A. Fotopoulos, N. Fournier, J. -D. Franc, J. Franco, S. Frasca, S. Frasconi, F. Frede, M. Frei, M. A. Frei, Z. Freise, A. Frey, R. Fricke, T. T. Friedrich, D. Fritschel, P. Frolov, V. V. Fujimoto, M. -K. Fulda, P. J. Fyffe, M. Gair, J. Galimberti, M. Gammaitoni, L. Garcia, J. Garufi, F. Gaspar, M. E. Gelencser, G. Gemme, G. Genin, E. Gennai, A. Gergely, L. A. Ghosh, S. Giaime, J. A. Giampanis, S. Giardina, K. D. Giazotto, A. Gil-Casanova, S. Gill, C. Gleason, J. Goetz, E. Gonzalez, G. Gorodetsky, M. L. Gossler, S. Gouaty, R. Graef, C. Graff, P. B. Granata, M. Grant, A. Gray, C. Greenhalgh, R. J. S. Gretarsson, A. M. Griffo, C. Grote, H. Grover, K. Grunewald, S. Guidi, G. M. Guido, C. Gupta, R. Gustafson, E. K. Gustafson, R. Hallam, J. M. Hammer, D. Hammond, G. Hanks, J. Hanna, C. Hanson, J. Harms, J. Harry, G. M. Harry, I. W. Harstad, E. D. Hartman, M. T. Haughian, K. Hayama, K. Hayau, J. -F. Heefner, J. Heidmann, A. Heintze, M. C. Heitmann, H. Hello, P. Hemming, G. Hendry, M. A. Heng, I. S. Heptonstall, A. W. Herrera, V. Heurs, M. Hewitson, M. Hild, S. Hoak, D. Hodge, K. A. Holt, K. Holtrop, M. Hong, T. Hooper, S. Hough, J. Howell, E. J. Hughey, B. Husa, S. Huttner, S. H. Huynh-Dinh, T. Ingram, D. R. Inta, R. Isogai, T. Ivanov, A. Izumi, K. Jacobson, M. James, E. Jang, Y. J. Jaranowski, P. Jesse, E. Johnson, W. W. Jones, D. I. Jones, R. Jonker, R. J. G. Ju, L. Kalmus, P. Kalogera, V. Kandhasamy, S. Kang, G. Kanner, J. B. Kasprzack, M. Kasturi, R. Katsavounidis, E. Katzman, W. Kaufer, H. Kaufman, K. Kawabe, K. Kawamura, S. Kawazoe, F. Keitel, D. Kelley, D. Kells, W. Keppel, D. G. Keresztes, Z. Khalaidovski, A. Khalili, F. Y. Khazanov, E. A. Kim, B. K. Kim, C. Kim, H. Kim, K. Kim, N. Kim, Y. M. King, P. J. Kinzel, D. L. Kissel, J. S. Klimenko, S. Kline, J. Kokeyama, K. Kondrashov, V. Koranda, S. Korth, W. Z. Kowalska, I. Kozak, D. Kringel, V. Krishnan, B. Krolak, A. Kuehn, G. Kumar, P. Kumar, R. Kurdyumov, R. Kwee, P. Lam, P. K. Landry, M. Langley, A. Lantz, B. Lastzka, N. Lawrie, C. Lazzarini, A. Le Roux, A. Leaci, P. Lee, C. H. Lee, H. K. Lee, H. M. Leong, J. R. Leonor, I. Leroy, N. Letendre, N. Lhuillier, V. Li, J. Li, T. G. F. Lindquist, P. E. Litvine, V. Liu, Y. Liu, Z. Lockerbie, N. A. Lodhia, D. Logue, J. Lorenzini, M. Loriette, V. Lormand, M. Losurdo, G. Lough, J. Lubinski, M. Lueck, H. Lundgren, A. P. Macarthur, J. Macdonald, E. Machenschalk, B. MacInnis, M. Macleod, D. M. Mageswaran, M. Mailand, K. Majorana, E. Maksimovic, I. Malvezzi, V. Man, N. Mandel, I. Mandic, V. Mantovani, M. Marchesoni, F. Marion, F. Marka, S. Marka, Z. Markosyan, A. Maros, E. Marque, J. Martelli, F. Martin, I. W. Martin, R. M. Marx, J. N. Mason, K. Masserot, A. Matichard, F. Matone, L. Matzner, R. A. Mavalvala, N. Mazzolo, G. McCarthy, R. McClelland, D. E. McGuire, S. C. McIntyre, G. McIver, J. Meadors, G. D. Mehmet, M. Meier, T. Melatos, A. Melissinos, A. C. Mendell, G. Menendez, D. F. Mercer, R. A. Meshkov, S. Messenger, C. Meyer, M. S. Miao, H. Michel, C. Milano, L. Miller, J. Minenkov, Y. Mingarelli, C. M. F. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Moe, B. Mohan, M. Mohapatra, S. R. P. Moraru, D. Moreno, G. Morgado, N. Morgia, A. Mori, T. Morriss, S. R. Mosca, S. Mossavi, K. Mours, B. Mow-Lowry, C. M. Mueller, C. L. Mueller, G. Mukherjee, S. Mullavey, A. Mueller-Ebhardt, H. Munch, J. Murphy, D. Murray, P. G. Mytidis, A. Nash, T. Naticchioni, L. Necula, V. Nelson, J. Neri, I. Newton, G. Nguyen, T. Nishizawa, A. Nitz, A. Nocera, F. Nolting, D. Normandin, M. E. Nuttall, L. Ochsner, E. O'Dell, J. Oelker, E. Ogin, G. H. Oh, J. J. Oh, S. H. Oldenberg, R. G. O'Reilly, B. O'Shaughnessy, R. Osthelder, C. Ott, C. D. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Page, A. Palladino, L. Palomba, C. Pan, Y. Pankow, C. Paoletti, F. Paoletti, R. Papa, M. A. Parisi, M. Pasqualetti, A. Passaquieti, R. Passuello, D. Pedraza, M. Penn, S. Perreca, A. Persichetti, G. Phelps, M. Pichot, M. Pickenpack, M. Piergiovanni, F. Pierro, V. Pihlaja, M. Pinard, L. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Poggiani, R. Poeld, J. Postiglione, F. Poux, C. Prato, M. Predoi, V. Prestegard, T. Price, L. R. Prijatelj, M. Principe, M. Privitera, S. Prix, R. Prodi, G. A. Prokhorov, L. G. Puncken, O. Punturo, M. Puppo, P. Quetschke, V. Quitzow-James, R. Raab, F. J. Rabeling, D. S. Racz, I. Radkins, H. Raffai, P. Rakhmanov, M. Ramet, C. Rankins, B. Rapagnani, P. Raymond, V. Re, V. Reed, C. M. Reed, T. Regimbau, T. Reid, S. Reitze, D. H. Ricci, F. Riesen, R. Riles, K. Roberts, M. Robertson, N. A. Robinet, F. Robinson, C. Robinson, E. L. Rocchi, A. Roddy, S. Rodriguez, C. Rodruck, M. Rolland, L. Rollins, J. G. Romano, J. D. Romano, R. Romie, J. H. Rosinska, D. Roever, C. Rowan, S. Ruediger, A. Ruggi, P. Ryan, K. Salemi, F. Sammut, L. Sandberg, V. Sankar, S. Sannibale, V. Santamaria, L. Santiago-Prieto, I. Santostasi, G. Saracco, E. Sassolas, B. Sathyaprakash, B. S. Saulson, P. R. Savage, R. L. Schilling, R. Schnabel, R. Schofield, R. M. S. Schulz, B. Schutz, B. F. Schwinberg, P. Scott, J. Scott, S. M. Seifert, F. Sellers, D. Sentenac, D. Sergeev, A. Shaddock, D. A. Shaltev, M. Shapiro, B. Shawhan, P. Shoemaker, D. H. Sidery, T. L. Siemens, X. Sigg, D. Simakov, D. Singer, A. Singer, L. Sintes, A. M. Skelton, G. R. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, R. J. E. Smith-Lefebvre, N. D. Somiya, K. Sorazu, B. Speirits, F. C. Sperandio, L. Stefszky, M. Steinert, E. Steinlechner, J. Steinlechner, S. Steplewski, S. Stochino, A. Stone, R. Strain, K. A. Strigin, S. E. Stroeer, A. S. Sturani, R. Stuver, A. L. Summerscales, T. Z. Sung, M. Susmithan, S. Sutton, P. J. Swinkels, B. Szeifert, G. Tacca, M. Taffarello, L. Talukder, D. Tanner, D. B. Tarabrin, S. P. Taylor, R. ter Braack, A. P. M. Thomas, P. Thorne, K. A. Thorne, K. S. Thrane, E. Thuering, A. Titsler, C. Tokmakov, K. V. Tomlinson, C. Toncelli, A. Tonelli, M. Torre, O. Torres, C. V. Torrie, C. I. Tournefier, E. Travasso, F. Traylor, G. Tse, M. Ugolini, D. Vahlbruch, H. Vajente, G. van den Brand, J. F. J. Van den Broeck, C. van der Putten, S. van Veggel, A. A. Vass, S. Vasuth, M. Vaulin, R. Vavoulidis, M. Vecchio, A. Vedovato, G. Veitch, J. Veitch, P. J. Venkateswara, K. Verkindt, D. Vetrano, F. Vicere, A. Villar, A. E. Vinet, J. -Y. Vitale, S. Vocca, H. Vorvick, C. Vyatchanin, S. P. Wade, A. Wade, L. Wade, M. Waldman, S. J. Wallace, L. Wan, Y. Wang, M. Wang, X. Wanner, A. Ward, R. L. Was, M. Weinert, M. Weinstein, A. J. Weiss, R. Welborn, T. Wen, L. Wessels, P. West, M. Westphal, T. Wette, K. Whelan, J. T. Whitcomb, S. E. White, D. J. Whiting, B. F. Wiesner, K. Wilkinson, C. Willems, P. A. Williams, L. Williams, R. Willke, B. Wimmer, M. Winkelmann, L. Winkler, W. Wipf, C. C. Wiseman, A. G. Wittel, H. Woan, G. Wooley, R. Worden, J. Yablon, J. Yakushin, I. Yamamoto, H. Yamamoto, K. Yancey, C. C. Yang, H. Yeaton-Massey, D. Yoshida, S. Yvert, M. Zadrozny, A. Zanolin, M. Zendri, J. -P. Zhang, F. Zhang, L. Zhao, C. Zotov, N. Zucker, M. E. Zweizig, J. CA ANTARES Collaboration ANTARES Collaboration LIGO Sci Collaboration LIGO Sci Collaboration Virgo Collaboration TI A first search for coincident gravitational waves and high energy neutrinos using LIGO, Virgo and ANTARES data from 2007 SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE gravitational waves / experiments; neutrino astronomy ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; SUPERCONDUCTING COSMIC STRINGS; MAGNETAR GIANT FLARES; SCIENCE RUN; RELATIVISTIC JETS; POINT SOURCES; BLACK-HOLES; LOCAL-RATE; TELESCOPE AB We present the results of the first search for gravitational wave bursts associated with high energy neutrinos. Together, these messengers could reveal new, hidden sources that are not observed by conventional photon astronomy, particularly at high energy. Our search uses neutrinos detected by the underwater neutrino telescope ANTARES in its 5 line configuration during the period January - September 2007, which coincided with the fifth and first science runs of LIGO and Virgo, respectively. The LIGO-Virgo data were analysed for candidate gravitational-wave signals coincident in time and direction with the neutrino events. No significant coincident events were observed. We place limits on the density of joint high energy neutrino - gravitational wave emission events in the local universe, and compare them with densities of merger and core-collapse events. C1 [Adrian-Martinez, S.; Ardid, M.; Bou-Cabo, M.; Ferri, M.; Larosa, G.; Martinez-Mora, J. A.] Univ Politecn Valencia, Inst Invest Gestio Integrada Zones Costaneres IGI, Gandia 46730, Spain. [Al Samarai, I.; Aubert, J-J.; Bertin, V.; Brunner, J.; Busto, J.; Carr, J.; Charif, Z.; Core, L.; Costantini, H.; Coyle, P.; Curtil, C.; Dornic, D.; Ernenwein, J-P.; Escoffier, S.; Galata, S.; Hallewell, G.; Riviere, C.; Vallee, C.; Vecchi, M.] Aix Marseille Univ, CPPM, CNRS, IN2P3, Marseille, France. [Albert, A.; Drouhin, D.; Racca, C.] GRPHE Inst Univ Technol Colmar, F-68008 Colmar, France. [Andre, M.] Tech Univ Catalonia, Lab Appl Bioacoust, Barcelona 08800, Spain. [Anghinolfi, M.; Kulikovskiy, V.; Taiuti, M.; Chincarini, A.; Gemme, G.; Prato, M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy. [Anton, G.; Eberl, T.; Enzenhoefer, A.; Fehn, K.; Folger, F.; Fritsch, U.; Geyer, K.; Graf, K.; Herold, B.; Hoessl, J.; Kalekin, O.; Kappes, A.; Katz, U.; Kopper, C.; Lahmann, R.; Meli, A.; Motz, H.; Neff, M.; Richardt, C.; Richter, R.; Roensch, K.; Schmid, J.; Schnabel, J.; Schoeck, F.; Seitz, T.; Shanidze, R.; Spies, A.; Wagner, S.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Anvar, S.; Louis, F.] CEA Saclay, Direct Sci Mat, Inst Rech Fondamentales Univers, Serv Elect Detecteurs & Informat, F-91191 Gif Sur Yvette, France. [Albert, A.; Astraatmadja, T.; Bogazzi, C.; Bouwhuis, M. C.; Decowski, M. P.; Heijboer, A. J.; Hsu, C. C.; de Jong, M.; Kooijman, P.; Kopper, C.; Lim, G.; Palioselitis, D.; Petrovic, J.; Presani, E.; Reed, C.; Samtleben, D. F. E.; Steijger, J. J. M.; Visser, E.; Wijnker, G.; de Wolf, E.; Agathos, M.; Bauer, Th. S.; Beker, M. G.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Jonker, R. J. G.; Li, T. G. F.; Rabeling, D. S.; ter Braack, A. P. M.; van den Brand, J. F. J.; Van den Broeck, C.; van der Putten, S.; Vitale, S.] NIKHEF H, NL-1009 DB Amsterdam, Netherlands. [Baret, B.; Bouhou, B.; Creusot, A.; Donzaud, C.; Kouchner, A.; Moscoso, L.; Van Elewyck, V.; Barsuglia, M.; Buy, C.; Chassande-Mottin, E.; Ward, R. L.] Univ Paris Diderot, APC, CNRS IN2P3, CEA IRFU,Observ Paris,Sorbonne Paris Cite, F-75205 Paris, France. [Basa, S.; Marcelin, M.; Nezri, E.] LAM, Pole Etoile Site Chateau Gombert, F-13388 Marseille 13, France. [Biagi, S.; Cecchini, S.; Chiarusi, T.; Giacomelli, G.; Margiotta, A.; Spurio, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Biagi, S.; Giacomelli, G.; Margiotta, A.; Spurio, M.; Dergachev, V.] Univ Bologna, Dipartimento Fis, I-40127 Bologna, Italy. [Bigongiari, C.; Dornic, D.; Emanuele, U.; Gomez-Gonzalez, J. P.; Hernandez-Rey, J. J.; Lambard, G.; Mangano, S.; Ruiz-Rivas, J.; Sanchez-Losa, A.; Yepes, H.; Zornoza, J. D.; Zuniga, J.] CSIC Univ Valencia, IFIC Inst Fis Corpuscular, Valencia 46071, Spain. [Capone, A.; De Bonis, G.; Fermani, P.; Simeone, F.; Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy. [Albert, A.; Arloganu, C. C.; De Bonis, G.; Fermani, P.; Simeone, F.; Allocca, A.; Colla, A.; Colombini, M.; Conte, A.; Frasca, S.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Gay, P.; Guillard, G.] Univ Clermont Ferrand, Clermont Univ, CNRS IN2P3, Lab Phys Corpusculaire, F-63000 Clermont Ferrand, France. [Charvis, Ph.; Deschamps, A.; Hello, Y.] Univ Nice Sophia Antipolis, Geoazur, CNRS INSU, IRD,Observ Cote Azur, F-06235 Villefranche Sur Mer, France. [Charvis, Ph.; Deschamps, A.; Hello, Y.] Univ Paris 06, F-06235 Villefranche Sur Mer, France. [Circella, M.; Montaruli, T.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Coniglione, R.; Distefano, C.; Giordano, V.; Lattuada, D.; Piattelli, P.; Riccobene, G.; Sapienza, P.] Ist Nazl Fis Nucl, LNS, I-95123 Catania, Italy. [Dekeyser, I.; Fuda, J-L.; Lefevre, D.; Martini, S.; Robert, A.; Tamburini, C.] Aix Marseille Univ, MIO, F-13288 Marseille 9, France. [Dekeyser, I.; Fuda, J-L.; Lefevre, D.; Martini, S.; Robert, A.; Tamburini, C.] Univ Sud Toulon Var, CNRS INSU, IRD UM 110, F-83957 La Garde, France. [Donzaud, C.] Univ Paris 11, F-91405 Orsay, France. [Dorosti, Q.; Kavatsyuk, O.; Loehner, H.] Univ Groningen, KVI, NL-9747 AA Groningen, Netherlands. [Ferry, S.; Loucatos, S.; Moscoso, L.; Payet, K.; Schuller, J-P.; Schuessler, F.; Stolarczyk, Th.; Vallage, B.; Vernin, P.] CEA Saclay, Direct Sci Mat, Inst Rech Fondamentales Univers, Serv Phys Particules, F-91191 Gif Sur Yvette, France. [Flaminio, V.; Morganti, M.; Allocca, A.; Basti, A.; Bonelli, L.; Boschi, V.; Braccini, S.; Bradaschia, C.; Cella, G.; Colacino, C. N.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Mantovani, M.; Paoletti, F.; Paoletti, R.; Passaquieti, R.; Passuello, D.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Torre, O.; Vajente, G.] INFN, Sez Pisa, I-56127 Pisa, Italy. [Flaminio, V.; Allocca, A.; Basti, A.; Bonelli, L.; Colacino, C. N.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, Dipartimento Fis, I-56127 Pisa, Italy. [Hamal, M.] Univ Mohammed 1, Lab Phys Matter & Radiat, Oujda 6000, Morocco. [van Haren, H.; Bitossi, M.] Royal Netherlands Inst Sea Res NIOZ, NL-1797 SZ Thorntje, Texel, Netherlands. [Kadler, M.; Kreykenbohm, I.; Wilms, J.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. [Kooijman, P.] Univ Utrecht, Fac Betawetenschappen, NL-3584 CC Utrecht, Netherlands. [Kooijman, P.; Lim, G.; de Wolf, E.] Univ Amsterdam, Inst Hoge Energie Fys, NL-1098 XG Amsterdam, Netherlands. [Kulikovskiy, V.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119991, Russia. [Lo Presti, D.; Russo, G. V.; Trovato, A.] INFN, Sez Catania, I-95125 Catania, Italy. [Lo Presti, D.; Russo, G. V.] Univ Catania, Dipartimento Fis & Astron, I-95125 Catania, Italy. [Montaruli, T.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [Pavalas, G. E.; Popa, V.; Rujoiu, M.] Inst Space Sci, R-77125 Bucharest, Magurele, Romania. [Pradier, T.] Univ Strasbourg, IPHC, F-67037 Strasbourg 2, France. [Pradier, T.] CNRS IN2P3, F-67037 Strasbourg 2, France. [Rostovtsev, A.; Zaborov, D.] ITEP, Moscow 117218, Russia. [Taiuti, M.] Univ Genoa, Dipartimento Fis, I-16146 Genoa, Italy. [Astraatmadja, T.; de Jong, M.] Leiden Univ, NL-2300 RA Leiden, Netherlands. [Morganti, M.] Accademia Navale Livorno, Livorno, Italy. [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C. B.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chalermsongsak, T.; Corsi, A.; Coyne, D. C.; Daudert, B.; Doravari, S.; Driggers, J. C.; Ehrens, P.; Engel, R.; Etzel, T.; Fotopoulos, N.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Lindquist, P. E.; Litvine, V.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Pedraza, M.; Poux, C.; Price, L. R.; Privitera, S.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Santamaria, L.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C. I.; Vass, S.; Villar, A. E.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T. D.; Griffo, C.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA. [Abernathy, M.; Barr, B.; Bassiri, R.; Bastarrika, M.; Bell, A. S.; Bell, C.; Beveridge, N.; Campsie, P.; Cumming, A.; Cunningham, L.; Edgar, M.; Evans, K.; Gill, C.; Grant, A.; Hammond, G.; Haughian, K.; Hendry, M. A.; Heng, I. S.; Hild, S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Logue, J.; Macarthur, J.; Macdonald, E.; Martin, I. W.; Murray, P. G.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Speirits, F. C.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland. [Accadia, T.; Bebronne, M.; Buskulic, D.; Dietz, A.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Tournefier, E.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS IN2P3, LAPP, F-74941 Annecy Le Vieux, France. [Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Forte, L. A.; Garufi, F.; Milano, L.; Mosca, S.; Parisi, M.; Persichetti, G.; Romano, R.] INFN, Sez Napoli, I-80126 Naples, Italy. [Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.; Mosca, S.; Parisi, M.; Persichetti, G.] Univ Naples Federico II, I-80126 Naples, Italy. [Acernese, F.; Addesso, P.; Barone, F.; Conte, R.; Postiglione, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy. [Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Bridges, D. O.; Cowart, M.; Evans, T.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Heintze, M. C.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Le Roux, A.; Lormand, M.; Meyer, M. S.; Nolting, D.; O'Reilly, B.; Overmier, H.; Ramet, C.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thorne, K. A.; Traylor, G.; Welborn, T.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA. [Adams, T.; Dent, T.; Edwards, M.; Fairhurst, S.; Macleod, D. M.; Messenger, C.; Nuttall, L.; Predoi, V.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Veitch, J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales. [Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, Milan, Italy. [Affeldt, C.; Allen, B.; Ast, S.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Damjanic, M.; Danzmann, K.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Heurs, M.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Lastzka, N.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Phelps, M.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Shaltev, M.; Simakov, D.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Thuering, A.; Vahlbruch, H.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkelmann, L.; Winkler, W.; Wittel, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Affeldt, C.; Allen, B.; Allocca, A.; Ast, S.; Aufmuth, P.; Aulbert, C.; Basti, A.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brillet, A.; Brinkmann, M.; Britzger, M.; Buonanno, A.; Dahl, K.; Damjanic, M.; Danzmann, K.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Heurs, M.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Lastzka, N.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Shaltev, M.; Simakov, D.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Thuering, A.; Vahlbruch, H.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkelmann, L.; Winkler, W.; Wittel, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Bulten, H. J.; Rabeling, D. S.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands. [Agatsuma, K.; Fujimoto, M. -K.; Hayama, K.; Izumi, K.; Kawamura, S.; Mori, T.; Nishizawa, A.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Allen, B.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Favata, M.; Giampanis, S.; Hammer, D.; Hughey, B.; Kline, J.; Koranda, S.; Mercer, R. A.; Moe, B.; Ochsner, E.; Oldenberg, R. G.; O'Shaughnessy, R.; Pankow, C.; Papa, M. A.; Siemens, X.; Skelton, G. R.; Wade, L.; Wade, M.; Wiseman, A. G.] Univ Wisconsin Milwaukee, Milwaukee, WI 53201 USA. [Allocca, A.; Paoletti, R.; Torre, O.] Univ Siena, I-53100 Siena, Italy. [Amariutei, D.; Bao, Y.; Ciani, G.; Feldbaum, D.; Gleason, J.; Hartman, M. T.; Klimenko, S.; Liu, Z.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Tanner, D. B.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA. [Atkinson, D.; Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Bland, B.; Clara, F.; Cook, D.; Garcia, J.; Gray, C.; Hanks, J.; Ingram, D. R.; Kawabe, K.; Landry, M.; Lhuillier, V.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R. L.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA. [Aylott, B. E.; Bond, C.; Carbone, L.; Cruise, A. M.; Cutler, R. M.; Freise, A.; Fulda, P. J.; Grover, K.; Hallam, J. M.; Lodhia, D.; Mandel, I.; Mingarelli, C. M. F.; Page, A.; Sidery, T. L.; Smith, R. J. E.; Vecchio, A.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Babak, S.; Behnke, B.; Grunewald, S.; Krishnan, B.; Leaci, P.; Papa, M. A.; Robinson, E. L.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Baker, P.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA. [Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cuoco, E.; Dattilo, V.; Day, R.; Ferrini, F.; Fiori, I.; Genin, E.; Hemming, G.; Kasprzack, M.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Ruggi, P.; Sentenac, D.; Swinkels, B.; Tacca, M.] EGO, I-56021 Cascina, PI, Italy. [Ballmer, S.; Brown, D. A.; Couvares, P.; Fisher, R. P.; Harry, I. W.; Kelley, D.; Kumar, P.; Lough, J.; Nitz, A.; Perreca, A.; Saulson, P. R.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA. [Barsotti, L.; Bodiya, T. P.; Corbitt, T. R.; Donovan, F.; Dwyer, S.; Evans, M.; Foley, S.; Fritschel, P.; Katsavounidis, E.; Kissel, J. S.; Kwee, P.; MacInnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Oelker, E.; Sankar, S.; Shapiro, B.; Shoemaker, D. H.; Smith-Lefebvre, N. D.; Vaulin, R.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zucker, M. E.] LIGO Massachusetts Inst Technol, Cambridge, MA 02139 USA. [Bartos, I.; Belopolski, I.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D.; Raffai, P.; Tse, M.] Columbia Univ, New York, NY 10027 USA. [Bassiri, R.; Beck, D.; Bhadbade, T.; Byer, R. L.; Clark, D. E.; Debra, D.; Herrera, V.; Kim, N.; Kurdyumov, R.; Lantz, B.; Markosyan, A.; Roberts, M.] Stanford Univ, Stanford, CA 94305 USA. [Krolak, A.] IM PAN, PL-00956 Warsaw, Poland. [Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland. [Bejger, M.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland. [Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland. [Krolak, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland. [Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland. [Benacquista, M.; Biswas, R.; Cagnoli, G.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Stroeer, A. S.; Torres, C. V.] Univ Texas Brownsville, Brownsville, TX 78520 USA. [Beyersdorf, P. T.; Cordier, M.] San Jose State Univ, San Jose, CA 95192 USA. [Bilenko, I. A.; Braginsky, V. B.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L. G.; Strigin, S. E.; Vyatchanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia. [Bizouard, M. A.; Brisson, V.; Cavalier, F.; Davier, M.; Franco, S.; Hello, P.; Kasprzack, M.; Leroy, N.; Robinet, F.; Vavoulidis, M.; Was, M.] Univ Paris 11, LAL, IN2P3, CNRS, F-91898 Orsay, France. [Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France. [Blackburn, L.; Camp, J. B.; Kanner, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blair, D.; Chen, X.; Chung, S.; Coward, D. M.; Danilishin, S. L.; Dumas, J. -C.; Hooper, S.; Howell, E. J.; Ju, L.; Susmithan, S.; Wen, L.; Whitcomb, S. E.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia. [Bondarescu, R.; Finn, L. S.; Menendez, D. F.; Owen, B. J.; Titsler, C.] Penn State Univ, University Pk, PA 16802 USA. [Brillet, A.; Cleva, F.; Coulon, J. -P.; Fournier, J. -D.; Heitmann, H.; Man, N.; Pichot, M.; Regimbau, T.; Vinet, J. -Y.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France. [Bondu, F.; Hayau, J. -F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France. [Bonnand, R.; Cagnoli, G.; Degallaix, J.; Flaminio, R.; Franc, J.; Galimberti, M.; Granata, M.; Michel, C.; Morgado, N.; Pinard, L.; Saracco, E.; Sassolas, B.] Univ Lyon 1, CNRS, IN2P3, LMA, F-69622 Villeurbanne, Lyon, France. [Bose, S.; Dayanga, T.; Ghosh, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA. [Bosi, L.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] INFN, Sez Perugia, I-06123 Perugia, Italy. [Gammaitoni, L.; Neri, I.; Travasso, F.] Univ Perugia, I-06123 Perugia, Italy. [Branchesi, M.; Guidi, G. M.; Lorenzini, M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] INFN, Sez Firenze, I-50019 Sesto Fiorentino, Italy. [Branchesi, M.; Cesarini, E.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy. [Brau, J. E.; Frey, R.; Harstad, E. D.; Leonor, I.; Quitzow-James, R.; Schofield, R. M. S.] Univ Oregon, Eugene, OR 97403 USA. [Briant, T.; Cohadon, P. -F.; Heidmann, A.] Univ Paris 06, CNRS, ENS, Lab Kastler Brossel, F-75005 Paris, France. [Capano, C. D.; Kanner, J. B.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA. [Buonanno, A.; Burguet-Castell, J.; Gil-Casanova, S.; Husa, S.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma De Mallorca, Spain. [Cadonati, L.; Clark, J. A.; Hoak, D.; McIver, J.; Mohapatra, S. R. P.] Univ Massachusetts Amherst, Amherst, MA 01003 USA. [Cannon, K.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Cao, J.; Chen, W.; Du, Z.; Li, J.; Liu, Y.; Wan, Y.; Wang, X.; Zhang, F.] Tsinghua Univ, Beijing 100084, Peoples R China. [Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.] Univ Michigan, Ann Arbor, MI 48109 USA. [Caudill, S.; Costa, C. A.; DeRosa, R.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Kokeyama, K.; Mullavey, A.; Slutsky, J.; Sung, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Cavaglia, M.; Dietz, A.; Rankins, B.] Univ Mississippi, University, MS 38677 USA. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Chen, Y.; Hong, T.; Kaufman, K.; Miao, H.; Ott, C. D.; Somiya, K.; Thorne, K. S.; Wen, L.; Yang, H.] Caltech CaRT, Pasadena, CA 91125 USA. [Cho, H. S.; Kim, Y. M.; Lee, C. H.] Pusan Natl Univ, Pusan 609735, South Korea. [Chow, J.; Chua, S. S. Y.; Inta, R.; Lam, P. K.; McClelland, D. E.; Miller, J.; Mow-Lowry, C. M.; Mullavey, A.; Nguyen, T.; Scott, S. M.; Shaddock, D. A.; Slagmolen, B. J. J.; Stefszky, M.; Wade, A.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Christensen, N.; Coughlin, M.; Isogai, T.] Carleton Coll, Northfield, MN 55057 USA. [Chung, C. T. Y.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia. [Coccia, E.; D'Antonio, S.; Emilio, M. Di Paolo; Fafone, V.; Malvezzi, V.; Minenkov, Y.; Morgia, A.; Palladino, L.; Re, V.; Rocchi, A.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Coccia, E.; Fafone, V.; Morgia, A.; Re, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy. [Emilio, M. Di Paolo; Palladino, L.] Univ Aquila, I-67100 Laquila, Italy. [Costa, C. A.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England. [Debreczeni, G.; Endroczi, G.; Gaspar, M. E.; Racz, I.; Vasuth, M.] RMKI, Wigner RCP, H-1121 Budapest, Hungary. [Dhurandhar, S.; Gupta, R.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Dorsher, S.; Kandhasamy, S.; Mandic, V.; Pihlaja, M.; Prestegard, T.; Thrane, E.] Univ Minnesota, Minneapolis, MN 55455 USA. [Drago, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Povo, Trento, Italy. [Drago, M.; Prodi, G. A.; Yamamoto, K.] Univ Trento, I-38050 Povo, Trento, Italy. [Taffarello, L.; Vedovato, G.; Zendri, J. -P.] INFN, Sez Padova, I-35131 Padua, Italy. [Yamamoto, K.] Univ Padua, I-35131 Padua, Italy. [Drever, R. W. P.; Harms, J.; Langley, A.] CALTECH, Pasadena, CA 91125 USA. [Farr, B. F.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Raymond, V.; Rodriguez, C.; Yablon, J.] Northwestern Univ, Evanston, IL 60208 USA. [Frei, M. A.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA. [Frei, Z.; Gelencser, G.; Raffai, P.; Szeifert, G.] Eotvos Lorand Univ, H-1117 Budapest, Hungary. [Gair, J.; Graff, P. B.] Univ Cambridge, Cambridge CB2 1TN, England. [Gergely, L. A.; Keresztes, Z.] Univ Szeged, H-6720 Szeged, Hungary. [Greenhalgh, R. J. S.; O'Dell, J.] HSIC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Gretarsson, A. M.; Jesse, E.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Hanna, C.] Perimeter Inst Theoret Phys, Toronto, ON N2L 2Y5, Canada. [Harry, G. M.] American Univ, Washington, DC 20016 USA. [Holtrop, M.] Univ New Hampshire, Durham, NH 03824 USA. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Kang, G.; Kim, B. K.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea. [Kasturi, R.; Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Kim, C.] Lund Observ, SE-22100 Lund, Sweden. [Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea. [Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea. [Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA. [McGuire, S. C.] Southern Univ & A&M Coll, Baton Rouge, LA 70813 USA. [Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA. [Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia. [Oh, J. J.; Oh, S. H.] Natl Inst Math Sci, Taejon 305390, South Korea. [Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA. [Santostasi, G.] McNeese State Univ, Lake Charles, LA 70609 USA. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA. [Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. RP Adrian-Martinez, S (reprint author), Univ Politecn Valencia, Inst Invest Gestio Integrada Zones Costaneres IGI, C Paranimf 1, Gandia 46730, Spain. EM Irene.DiPalma@aei.mpg.de; thierry.pradier@iphc.cnrs.fr RI Howell, Eric/H-5072-2014; Costa, Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Ward, Robert/I-8032-2014; Frasconi, Franco/K-1068-2016; Charvis, Philippe/K-1576-2016; Simeone, Francesco/L-1057-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Prato, Mirko/D-8531-2012; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Lo Presti, Domenico/G-2709-2013; Cesarini, Elisabetta/C-4507-2017; Ardid, Miguel/H-9544-2015; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Strain, Kenneth/D-5236-2011; Trovato, Agata/F-4160-2016; Biagi, Simone/G-4557-2016; Heidmann, Antoine/G-4295-2016; Distefano, Carla/G-5213-2016; Bao, Yiliang/G-9848-2016; Riccobene, Giorgio Maria/A-4502-2010; Ott, Christian/G-2651-2011; mosca, simona/I-7116-2012; Eberl, Thomas/J-4826-2016; Hernandez-Rey, Juan Jose/N-5955-2014; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Neri, Igor/F-1482-2010; cabo, bou/N-2076-2014; Shaddock, Daniel/A-7534-2011; Postiglione, Fabio/O-4744-2015; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martinez-Mora, Juan Antonio/P-3552-2015; Martelli, Filippo/P-4041-2015; Piattelli, Paolo/J-2958-2012; Canuel, Benjamin/C-7459-2014; Capone, Antonio/F-1098-2010; Schussler, Fabian/G-5313-2013; Lee, Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; McClelland, David/E-6765-2010; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Brunner, Juergen/G-3540-2015; Finn, Lee Samuel/A-3452-2009; Anton, Gisela/C-4840-2013; Zuniga, Juan/P-4385-2014; Sigg, Daniel/I-4308-2015; Salemi, Francesco/F-6988-2014; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov, Valery/D-8501-2012; Bell, Angus/E-7312-2011; Bilenko, Igor/D-5172-2012; Kumar, Prem/B-6691-2009; Vecchi, Manuela/J-9180-2014; Losurdo, Giovanni/K-1241-2014; Lam, Ping Koy/A-5276-2008; Zornoza, Juan de Dios/L-1604-2014; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Katz, Uli/E-1925-2013; Lohner, Herbert/B-2397-2014; Khazanov, Efim/B-6643-2014; prodi, giovanni/B-4398-2010; Gemme, Gianluca/C-7233-2008; Wilms, Joern/C-8116-2013; Prokhorov, Leonid/I-2953-2012; Gammaitoni, Luca/B-5375-2009; Steinlechner, Sebastian/D-5781-2013; Miao, Haixing/O-1300-2013; Parisi, Maria/D-2817-2013; Marchesoni, Fabio/A-1920-2008; OI Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Hallam, Jonathan Mark/0000-0002-7087-0461; Vetrano, Flavio/0000-0002-7523-4296; Naticchioni, Luca/0000-0003-2918-0730; Milano, Leopoldo/0000-0001-9487-5876; Hsu, Ching-Cheng/0000-0001-9406-2023; Papa, M.Alessandra/0000-0002-1007-5298; Aulbert, Carsten/0000-0002-1481-8319; Ferri Garcia, Marcelino/0000-0002-2049-3821; Pinto, Innocenzo M./0000-0002-2679-4457; Escoffier, Stephanie/0000-0002-2847-7498; Farr, Ben/0000-0002-2916-9200; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Howell, Eric/0000-0001-7891-2817; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Jaranowski, Piotr/0000-0001-8085-3414; Swinkels, Bas/0000-0002-3066-3601; Spurio, Maurizio/0000-0002-8698-3655; Ward, Robert/0000-0001-5503-5241; Frasconi, Franco/0000-0003-4204-6587; Charvis, Philippe/0000-0003-4397-7842; Ferrante, Isidoro/0000-0002-0083-7228; Prato, Mirko/0000-0002-2188-8059; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Lo Presti, Domenico/0000-0002-4540-2885; Cesarini, Elisabetta/0000-0001-9127-3167; Ardid, Miguel/0000-0002-3199-594X; Nitz, Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Husa, Sascha/0000-0002-0445-1971; Di Paolo Emilio, Maurizio/0000-0002-9558-3610; Vitale, Salvatore/0000-0003-2700-0767; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Kanner, Jonah/0000-0001-8115-0577; PERSICHETTI, GIANLUCA/0000-0001-8424-9791; Kadler, Matthias/0000-0001-5606-6154; Freise, Andreas/0000-0001-6586-9901; Gehring, Tobias/0000-0002-4311-2593; Strain, Kenneth/0000-0002-2066-5355; Trovato, Agata/0000-0002-9714-1904; Biagi, Simone/0000-0001-8598-0017; Heidmann, Antoine/0000-0002-0784-5175; Distefano, Carla/0000-0001-8632-1136; Riccobene, Giorgio Maria/0000-0002-0600-2774; Ott, Christian/0000-0003-4993-2055; mosca, simona/0000-0001-7869-8275; Eberl, Thomas/0000-0002-5301-9106; Hernandez-Rey, Juan Jose/0000-0002-1527-7200; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Neri, Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494; Postiglione, Fabio/0000-0003-0628-3796; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martinez-Mora, Juan Antonio/0000-0001-7956-2847; Martelli, Filippo/0000-0003-3761-8616; O'Shaughnessy, Richard/0000-0001-5832-8517; Presani, Eleonora/0000-0001-6254-9603; Vocca, Helios/0000-0002-1200-3917; Fairhurst, Stephen/0000-0001-8480-1961; Addesso, Paolo/0000-0003-0895-184X; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Sanchez Losa, Agustin/0000-0001-9596-7078; Bigongiari, Ciro/0000-0003-3293-8522; Nishizawa, Atsushi/0000-0003-3562-0990; Piattelli, Paolo/0000-0003-4748-6485; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; Schussler, Fabian/0000-0003-1500-6571; Lee, Chang-Hwan/0000-0003-3221-1171; McClelland, David/0000-0001-6210-5842; Vecchio, Alberto/0000-0002-6254-1617; Brunner, Juergen/0000-0002-5052-7236; Finn, Lee Samuel/0000-0002-3937-0688; Anton, Gisela/0000-0003-2039-4724; Zuniga, Juan/0000-0002-1041-6451; Sigg, Daniel/0000-0003-4606-6526; Gorodetsky, Michael/0000-0002-5159-2742; Bell, Angus/0000-0003-1523-0821; Losurdo, Giovanni/0000-0003-0452-746X; Lam, Ping Koy/0000-0002-4421-601X; Zornoza, Juan de Dios/0000-0002-1834-0690; Danilishin, Stefan/0000-0001-7758-7493; Katz, Uli/0000-0002-7063-4418; Lohner, Herbert/0000-0002-7441-739X; prodi, giovanni/0000-0001-5256-915X; Gemme, Gianluca/0000-0002-1127-7406; Wilms, Joern/0000-0003-2065-5410; Gammaitoni, Luca/0000-0002-4972-7062; Steinlechner, Sebastian/0000-0003-4710-8548; Miao, Haixing/0000-0003-4101-9958; Marchesoni, Fabio/0000-0001-9240-6793; Principe, Maria/0000-0002-6327-0628 FU United States National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter; Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation; Centre National de la Recherche Scientifique (CNRS); Commissariat a l'energie atomique et aux energies alternatives (CEA); Agence National de la Recherche (ANR); Commission Europeenne (FEDER fund and Marie Curie Program); Region Alsace (contrat CPER); Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Stichting voor Fundamenteel Onderzoek der Materie (FOM), the Netherlands; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Ciencia e Innovacion (MICINN), Spain; Prometeo of Generalitat Valenciana (GVA), Spain; Multi-Dark, Spain FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation.; The authors also acknowledge the financial support of the funding agencies for the construction and operation of the ANTARES neutrino telescope: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Agence National de la Recherche (ANR), Commission Europeenne (FEDER fund and Marie Curie Program), Region Alsace (contrat CPER), Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Stichting voor Fundamenteel Onderzoek der Materie (FOM), Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Ciencia e Innovacion (MICINN), Prometeo of Generalitat Valenciana (GVA) and Multi-Dark, Spain. They also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities. This publication has been assigned LIGO Document Number LIGO-P1200006. NR 153 TC 11 Z9 11 U1 6 U2 101 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD JUN PY 2013 IS 6 AR 008 DI 10.1088/1475-7516/2013/06/008 PG 40 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 175AB UT WOS:000321200100008 ER PT J AU Chen, Y Velicogna, I Famiglietti, JS Randerson, JT AF Chen, Yang Velicogna, Isabella Famiglietti, James S. Randerson, James T. TI Satellite observations of terrestrial water storage provide early warning information about drought and fire season severity in the Amazon SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE wildfire; deforestation; soil moisture recharge; teleconnection; Tropical Rain Measuring Mission (TRMM); Atmospheric Infrared Sounder (AIRS) ID EL-NINO; SOUTHERN-OSCILLATION; SURFACE TEMPERATURES; CLIMATE; FOREST; MODIS; DEFORESTATION; GRACE; BASIN; PRECIPITATION AB Fire risk in the Amazon can be predicted several months before the onset of the dry season using sea surface temperatures in the tropical north Atlantic and tropical Pacific. The lead times between ocean state and the period of maximum burning (4-11 months) may enable the development of forecasts with benefits for forest conservation, yet the underlying physical and biological mechanisms responsible for these temporal offsets are not well known. Here, we examined the hypothesis that year-to-year variations in soil water recharge during the wet season modify atmospheric water vapor and fire behavior during the following dry season. We tested this hypothesis by analyzing terrestrial water storage observations from the Gravity Recovery and Climate Experiment (GRACE), active fires from the Moderate Resolution Imaging Spectroradiometer (MODIS), and several other satellite and atmospheric reanalysis datasets during 2002-2011. We found that terrestrial water storage deficits preceded severe fire seasons across the southern Amazon. The most significant relationships between monthly terrestrial water storage and the sum of active fires during the dry season occurred during April-August (p<0.02), corresponding to 1-5 month lead times before the peak month of burning (September). Analysis of other datasets provided evidence for a cascade of processes during drought events, with lower cumulative precipitation (and higher cumulative evapotranspiration) in the wet season substantially reducing terrestrial water storage, and subsequently, surface and column atmospheric water vapor. Our results suggest that terrestrial water storage observations from GRACE have the potential to improve fire season forecasts for the southern Amazon. C1 [Chen, Yang; Velicogna, Isabella; Famiglietti, James S.; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Velicogna, Isabella] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Chen, Y (reprint author), Univ Calif Irvine, 2101C Croul Hall, Irvine, CA 92697 USA. EM yang.chen@uci.edu FU NASA [NNX11AF96G]; Atmosphere, Cryosphere, Hydrology, and Interdisciplinary Science (IDS) programs [NNX10AT83G]; National Science Foundation [AGS-1048890]; Gordon and Betty Moore Foundation [GBMF 3269] FX This work was supported by NASA Carbon Cycle (NNX11AF96G), Atmosphere (NNX10AT83G), Cryosphere, Hydrology, and Interdisciplinary Science (IDS) programs, the National Science Foundation (AGS-1048890), and the Gordon and Betty Moore Foundation (GBMF 3269). NR 68 TC 20 Z9 20 U1 2 U2 43 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUN PY 2013 VL 118 IS 2 BP 495 EP 504 DI 10.1002/jgrg.20046 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 224TU UT WOS:000324913100011 ER PT J AU Scott-Denton, LE Moore, DJP Rosenbloom, NA Kittel, TGF Burns, SP Schimel, DS Monson, RK AF Scott-Denton, Laura E. Moore, David J. P. Rosenbloom, Nan A. Kittel, Timothy G. F. Burns, Sean P. Schimel, David S. Monson, Russell K. TI Forecasting net ecosystem CO2 exchange in a subalpine forest using model data assimilation combined with simulated climate and weather generation SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE warming; carbon cycle; sequestration ID DAILY SOLAR-RADIATION; WATER-USE EFFICIENCY; HIGH-ELEVATION; TERRESTRIAL ECOSYSTEMS; DATA FUSION; DAILY PRECIPITATION; CIRCULATION MODEL; CARBON SINK; FLUXES; FUTURE AB Forecasting the carbon uptake potential of terrestrial ecosystems in the face of future climate change has proven challenging. Process models, which have been increasingly used to study ecosystem-atmosphere carbon and water exchanges when conditioned with tower-based eddy covariance data, have the potential to inform us about biogeochemical processes in future climate regimes, but only if we can reconcile the spatial and temporal scales used for observed fluxes and projected climate. Here, we used weather generator and ecosystem process models conditioned on observed weather dynamics and carbon/water fluxes, and embedded them within climate projections from a suite of six Earth Systems Models. Using this combination of models, we studied carbon cycle processes in a subalpine forest within the context of future (2080-2099) climate regimes. The assimilation of daily averaged, observed net ecosystem CO2 exchange (NEE) and evapotranspiration (ET) into the ecosystem process model resulted in retrieval of projected NEE with a level of accuracy that was similar to that following the assimilation of half-daily averaged observations; the assimilation of 30min averaged fluxes or monthly averaged fluxes caused degradation in the model's capacity to accurately simulate seasonal patterns in observed NEE. Using daily averaged flux data with daily averaged weather data projected for the period 2080-2099, we predicted greater forest net CO2 uptake in response to a lengthening of the growing season. These results contradict our previous observations of reduced CO2 uptake in response to longer growing seasons in the current (1999-2008) climate regime. The difference between these analyses is due to a projected increase in the frequency of rain versus snow during warmer winters of the future. Our results demonstrate the sensitivity of modeled processes to local variation in meteorology, which is often left unresolved in traditional approaches to earth systems modeling, and the importance of maintaining similarity in the timescales used in ecosystem process models driven by downscaled climate projections. C1 [Scott-Denton, Laura E.; Monson, Russell K.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Moore, David J. P.; Monson, Russell K.] Univ Arizona, Sch Nat Resources & Environm, Tucson, AZ USA. [Rosenbloom, Nan A.; Burns, Sean P.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Kittel, Timothy G. F.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Burns, Sean P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Schimel, David S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Monson, Russell K.] Univ Arizona, Tree Ring Res Lab, Tucson, AZ 85721 USA. RP Scott-Denton, LE (reprint author), Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. EM laura_ontheweb@yahoo.com RI Burns, Sean/A-9352-2008; Moore, David/A-6268-2013 OI Burns, Sean/0000-0002-6258-1838; FU U.S. National Science Foundation [DEB-0743251]; U.S. Department of Energy [ER-65088] FX We are grateful to Kurt Chowanski, Mark Losleben, Lucas Zukiewicz, Kelly Matheson, Dave Millar, John Knowles, and Kirk Ranno for data collection at the Niwot Ridge C1 climate station. We thank the USDA Natural Resources Conservation Service, Colorado Snow Survey Program, for the SNOTEL network data. We thank Julie Arblaster and Gerald Meehl of the National Center for Atmospheric Research for providing ESM results for the spatial grids used in this analysis. We thank Sean Worthington for making the map in Figure 1. Diego Riveros-Iregui, John Zobitz, and Ankur Desai provided valuable discussions about the SIPNET modeling. This research was supported by the U.S. National Science Foundation (grant DEB-0743251) and the U.S. Department of Energy (grant ER-65088). NR 75 TC 6 Z9 6 U1 1 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUN PY 2013 VL 118 IS 2 BP 549 EP 565 DI 10.1002/jgrg.20039 PG 17 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 224TU UT WOS:000324913100014 ER PT J AU Yi, YH Kimball, JS Jones, LA Reichle, RH Nemani, R Margolis, HA AF Yi, Yonghong Kimball, John S. Jones, Lucas A. Reichle, Rolf H. Nemani, Ramakrishna Margolis, Hank A. TI Recent climate and fire disturbance impacts on boreal and arctic ecosystem productivity estimated using a satellite-based terrestrial carbon flux model SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE gross primary productivity; net ecosystem exchange; fire disturbance; high latitudes; satellite remote sensing ID NET PRIMARY PRODUCTION; GROSS PRIMARY PRODUCTION; SOIL ORGANIC-CARBON; CONSTANT FRACTION; DECIDUOUS FOREST; USE EFFICIENCY; RESPIRATION; EXCHANGE; DROUGHT; MODIS AB Warming and changing fire regimes in the northern (45 degrees N) latitudes have consequences for land-atmosphere carbon feedbacks to climate change. A terrestrial carbon flux model integrating satellite Normalized Difference Vegetation Index and burned area records with global meteorology data was used to quantify daily vegetation gross primary productivity (GPP) and net ecosystem CO2 exchange (NEE) over a pan-boreal/Arctic domain and their sensitivity to climate variability, drought, and fire from 2000 to 2010. Model validation against regional tower carbon flux measurements showed overall good agreement for GPP (47 sites: R=0.83, root mean square difference (RMSD)=1.93gCm(-2)d(-1)) and consistency for NEE (22 sites: R=0.56, RMSD=1.46gCm(-2)d(-1)). The model simulations also tracked post-fire NEE recovery indicated from three boreal tower fire chronosequence networks but with larger model uncertainty during early succession. Annual GPP was significantly (p<0.005) larger in warmer years than in colder years, except for Eurasian boreal forest, which showed greater drought sensitivity due to characteristic warmer, drier growing seasons relative to other areas. The NEE response to climate variability and fire was mitigated by compensating changes in GPP and respiration, though NEE carbon losses were generally observed in areas with severe drought or burning. Drought and temperature variations also had larger regional impacts on GPP and NEE than fire during the study period, though fire disturbances were heterogeneous, with larger impacts on carbon fluxes for some areas and years. These results are being used to inform development of similar operational carbon products for the NASA Soil Moisture Active Passive (SMAP) mission. C1 [Yi, Yonghong; Kimball, John S.; Jones, Lucas A.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. [Yi, Yonghong; Kimball, John S.; Jones, Lucas A.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Reichle, Rolf H.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA. [Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Margolis, Hank A.] Univ Laval, Fac Foresterie Geog & Geomat, Ctr Etud Foret, Quebec City, PQ, Canada. RP Yi, YH (reprint author), Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. EM yonghong.yi@ntsg.umt.edu RI Reichle, Rolf/E-1419-2012; Yi, Yonghong/C-2395-2017 FU NASA Terrestrial Ecology program [NNX09AP52G, NNX11AD46G]; CarboEuropeIP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National Science Foundation; University of Tuscia; Universite Laval and Environment Canada; US Department of Energy; NOAA ESRL FX We thank the Editor, Eric Kasischke, Richard Waring, and one anonymous reviewer for their constructive comments. This work was supported with funding from the NASA Terrestrial Ecology program (NNX09AP52G and NNX11AD46G). This work used eddy covariance data acquired by the FLUXNET community, which was supported by the CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for Biogeochemistry, National Science Foundation, University of Tuscia, Universite Laval and Environment Canada, US Department of Energy and NOAA ESRL, as well as many local funders including Global Change Research Centre AS Czech Republic, Wisconsin Focus on Energy, and Forest Department of the Autonomous Province of Bolzano-CO2-measuring station of Renon/Ritten. We thank Drs. K.J. Davis, P. Bolstad, A. E. Andrews, B. D. Cook, A. R. Desai, and many other PIs for sharing the flux tower data. NR 74 TC 12 Z9 14 U1 4 U2 61 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUN PY 2013 VL 118 IS 2 BP 606 EP 622 DI 10.1002/jgrg.20053 PG 17 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 224TU UT WOS:000324913100018 ER PT J AU Berry, J Wolf, A Campbell, JE Baker, I Blake, N Blake, D Denning, AS Kawa, SR Montzka, SA Seibt, U Stimler, K Yakir, D Zhu, ZX AF Berry, Joe Wolf, Adam Campbell, J. Elliott Baker, Ian Blake, Nicola Blake, Don Denning, A. Scott Kawa, S. Randy Montzka, Stephen A. Seibt, Ulrike Stimler, Keren Yakir, Dan Zhu, Zhengxin TI A coupled model of the global cycles of carbonyl sulfide and CO2: A possible new window on the carbon cycle SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE Carbonyl Sulfide; Carbon dioxide; PCTM; SiB ID STOMATAL CONDUCTANCE; CANOPY REFLECTANCE; ATMOSPHERIC CO2; GAS-EXCHANGE; LEAF MODELS; PHOTOSYNTHESIS; TRANSPIRATION; ANHYDRASE; LEAVES; FLUXES AB Carbonyl sulfide (COS) is an atmospheric trace gas that participates in some key reactions of the carbon cycle and thus holds great promise for studies of carbon cycle processes. Global monitoring networks and atmospheric sampling programs provide concurrent data on COS and CO2 concentrations in the free troposphere and atmospheric boundary layer over vegetated areas. Here we present a modeling framework for interpreting these data and illustrate what COS measurements might tell us about carbon cycle processes. We implemented mechanistic and empirical descriptions of leaf and soil COS uptake into a global carbon cycle model (SiB 3) to obtain new estimates of the COS land flux. We then introduced these revised boundary conditions to an atmospheric transport model (Parameterized Chemical Transport Model) to simulate the variations in the concentration of COS and CO2 in the global atmosphere. To balance the threefold increase in the global vegetation sink relative to the previous baseline estimate, we propose a new ocean COS source. Using a simple inversion approach, we optimized the latitudinal distribution of this ocean source and found that it is concentrated in the tropics. The new model is capable of reproducing the seasonal variation in atmospheric concentration at most background atmospheric sites. The model also reproduces the observed large vertical gradients in COS between the boundary layer and free troposphere. Using a simulation experiment, we demonstrate that comparing drawdown of CO2 with COS could provide additional constraints on differential responses of photosynthesis and respiration to environmental forcing. The separation of these two distinct processes is essential to understand the carbon cycle components for improved prediction of future responses of the terrestrial biosphere to changing environmental conditions. C1 [Berry, Joe] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Wolf, Adam] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Campbell, J. Elliott] Univ Calif, Sierra Nevada Res Inst, Merced, CA USA. [Baker, Ian; Denning, A. Scott] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Blake, Nicola; Blake, Don] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA. [Kawa, S. Randy; Zhu, Zhengxin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Montzka, Stephen A.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Seibt, Ulrike] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Stimler, Keren; Yakir, Dan] Weizmann Inst Sci, IL-76100 Rehovot, Israel. RP Berry, J (reprint author), Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. EM joeberry@stanford.edu RI Yakir, Dan/K-1500-2012 FU NASA Earth Science Program; Office of Science (BER), U. S. Department of Energy FX We gratefully acknowledge George Wolf and Orrick, Herrington & Sutcliffe LLP for providing a meeting space to develop this work and Mohammad Abu-Naser for helping in the preparation of figures. This research was supported in part by the NASA Earth Science Program and the Office of Science (BER), U. S. Department of Energy. This research also had substantial contributions that were conducted without grant support and reflect the generosity of our colleagues and home institutions. NR 55 TC 34 Z9 34 U1 3 U2 49 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUN PY 2013 VL 118 IS 2 BP 842 EP 852 DI 10.1002/jgrg.20068 PG 11 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 224TU UT WOS:000324913100034 ER PT J AU Parizek, BR Christianson, K Anandakrishnan, S Alley, RB Walker, RT Edwards, RA Wolfe, DS Bertini, GT Rinehart, SK Bindschadler, RA Nowicki, SMJ AF Parizek, B. R. Christianson, K. Anandakrishnan, S. Alley, R. B. Walker, R. T. Edwards, R. A. Wolfe, D. S. Bertini, G. T. Rinehart, S. K. Bindschadler, R. A. Nowicki, S. M. J. TI Dynamic (in)stability of Thwaites Glacier, West Antarctica SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article DE glaciers; glaciology; modeling; dynamics; subglacial processes; radar ID PINE ISLAND GLACIER; DIGITAL ELEVATION MODEL; SHELF-OCEAN INTERACTION; SHEET GROUNDING LINES; ICE-SHEET; SEA-LEVEL; SUBGLACIAL LAKES; MASS-BALANCE; FLOW SPEED; LASER DATA AB Thwaites Glacier, West Antarctica, has the potential to directly contribute approximate to 1m to sea level and currently is losing mass and thinning rapidly. Here, we report on regional results for the Sea-level Response to Ice Sheet Evolution (SeaRISE) experiments and investigate the impact of i) spatial resolution within existing data sets, ii) grounding-zone processes, and iii) till rheology on the dynamics of this outlet glacier. In addition to the SeaRISE data sets, we use detailed aerogeophysical and satellite data from Thwaites Glacier as input to a coupled ice stream/ice-shelf/ocean-plume model that includes oceanic influences across a several kilometers wide grounding zone suggested by new, high-resolution data. Our results indicate that the ice tongue provides limited stability, and that while future atmospheric warming will likely add mass to the surface of the glacier, strong ice stream stabilization on bedrock highs narrower than the length of the grounding zone may be ephemeral if circulating waters substantially reduce basal resistance and enhance melting beneath grounded ice within this zone. However, we find that stability is significantly enhanced by effectively plastic till beds. Accurate projections of future sea level change relies on correct understanding of the till rheology as well as local basal processes near the grounding line. C1 [Parizek, B. R.] Penn State Univ, Du Bois, PA 15801 USA. [Christianson, K.; Anandakrishnan, S.; Alley, R. B.; Walker, R. T.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Christianson, K.; Anandakrishnan, S.; Alley, R. B.; Walker, R. T.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. [Christianson, K.] St Olaf Coll, Dept Phys, Northfield, MN 55057 USA. [Walker, R. T.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Walker, R. T.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Edwards, R. A.] Penn State Univ, Dept Civil & Environm Engn, University Pk, PA 16802 USA. [Wolfe, D. S.] Penn State Univ, Dept Engn Sci & Mech, University Pk, PA 16802 USA. [Bertini, G. T.] Penn State Univ, Dept Ind & Mfg Engn, University Pk, PA 16802 USA. [Rinehart, S. K.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Bindschadler, R. A.; Nowicki, S. M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Parizek, BR (reprint author), Penn State Univ, Du Bois, PA 15801 USA. EM parizek@psu.edu FU NSF [0531211, 0632198, 0732844, 0758274, 0909335]; Center for Remote Sensing of Ice Sheets (CReSIS) [0424589]; NASA [NRA-04-OES-02, NNX-09-AV94G, NNX-10-AI04G, 10-CRYO10-0025]; NASA Cryospheric Science program [281945.02.53.02.19]; NSF graduate research fellowship FX This work was supported by NSF grants 0531211, 0632198, 0732844, 0758274, 0909335, the Center for Remote Sensing of Ice Sheets (CReSIS) 0424589, by NASA under grants NRA-04-OES-02, NNX-09-AV94G, NNX-10-AI04G, 10-CRYO10-0025, and the NASA Cryospheric Science program (Grant 281945.02.53.02.19), as well as an NSF graduate research fellowship (K. C.). We thank Operation IceBridge and the National Snow and Ice Data Center for access to aerogeophysical data and the SeaRISE community of scientists for all of the collaborative work over the past several years. Finally, we would like to recognize the efforts of the Scientific Editor, Bryn Hubbard, the Associate Editor, and two anonymous referees. Their critical reviews were invaluable. NR 85 TC 30 Z9 30 U1 2 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD JUN PY 2013 VL 118 IS 2 BP 638 EP 655 DI 10.1002/jgrf.20044 PG 18 WC Geosciences, Multidisciplinary SC Geology GA 225VU UT WOS:000324993900019 ER PT J AU Schlegel, NJ Larour, E Seroussi, H Morlighem, M Box, JE AF Schlegel, N. -J. Larour, E. Seroussi, H. Morlighem, M. Box, J. E. TI Decadal-scale sensitivity of Northeast Greenland ice flow to errors in surface mass balance using ISSM SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article DE Greenland; ice flow; sensitivity; surface mass balance; ice dynamics; ice stream ID SPATIAL-RESOLUTION; SHEET; CLIMATE; MODEL; ACCELERATION; ANTARCTICA; GLACIERS; STREAM; BASAL AB The behavior of the Greenland Ice Sheet, which is considered a major contributor to sea level changes, is best understood on century and longer time scales. However, on decadal time scales, its response is less predictable due to the difficulty of modeling surface climate, as well as incomplete understanding of the dynamic processes responsible for ice flow. Therefore, it is imperative to understand how modeling advancements, such as increased spatial resolution or more comprehensive ice flow equations, might improve projections of ice sheet response to climatic trends. Here we examine how a finely resolved climate forcing influences a high-resolution ice stream model that considers longitudinal stresses. We simulate ice flow using a two-dimensional Shelfy-Stream Approximation implemented within the Ice Sheet System Model (ISSM) and use uncertainty quantification tools embedded within the model to calculate the sensitivity of ice flow within the Northeast Greenland Ice Stream to errors in surface mass balance (SMB) forcing. Our results suggest that the model tends to smooth ice velocities even when forced with extreme errors in SMB. Indeed, errors propagate linearly through the model, resulting in discharge uncertainty of 16% or 1.9Gt/yr. We find that mass flux is most sensitive to local errors but is also affected by errors hundreds of kilometers away; thus, an accurate SMB map of the entire basin is critical for realistic simulation. Furthermore, sensitivity analyses indicate that SMB forcing needs to be provided at a resolution of at least 40km. C1 [Schlegel, N. -J.; Larour, E.; Seroussi, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Morlighem, M.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Box, J. E.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. RP Schlegel, NJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr MS 300-227, Pasadena, CA 91109 USA. EM schlegel@eps.berkeley.edu RI Morlighem, Mathieu/O-9942-2014; Box, Jason/H-5770-2013 OI Morlighem, Mathieu/0000-0001-5219-1310; FU National Aeronautics and Space Administration's Modeling, Analysis and Prediction (MAP) Program; NASA [NNX10AT68G]; NSF [ANT-0424589] FX This work was performed at the California Institute of Technology's Jet Propulsion Laboratory under a contract with the National Aeronautics and Space Administration's Modeling, Analysis and Prediction (MAP) Program. H. S. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. The authors would like to acknowledge the data provided by the National Snow and Ice Data Center DAAC, University of Colorado, Boulder, CO, Operation IceBridge, as well as CReSIS data generated from NSF grant ANT-0424589 and NASA grant NNX10AT68G. They also wish to thank John Schiermeier for the time he dedicated to the implementation of the DAKOTA-ISSM interface and for the helpful discussions regarding UQ methods. NR 62 TC 6 Z9 6 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD JUN PY 2013 VL 118 IS 2 BP 667 EP 680 DI 10.1002/jgrf.20062 PG 14 WC Geosciences, Multidisciplinary SC Geology GA 225VU UT WOS:000324993900021 ER PT J AU Borstad, CP McClung, DM AF Borstad, C. P. McClung, D. M. TI A higher-order method for determining quasi-brittle tensile fracture parameters governing the release of slab avalanches and a new tool for in situ indexing SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article DE quasi-brittle; avalanches; fracture mechanics; brittleness ID PROCESS ZONE LENGTH; SNOW; TOUGHNESS; STRENGTH; SIZE; ENERGY; ICE AB The tensile fracture of heterogeneous earth materials such as snow, ice, and rocks can be characterized by two fracture parametersthe fracture toughness and the fracture process zone length. The latter length scale characterizes the zone of microcracking surrounding a crack tip in a heterogeneous material. For alpine snow, these two fracture parameters influence the release dimensions and thus destructive potential of slab avalanches. In general, it is difficult to determine these parameters concurrently, and most experimental methods are based on first-order scaling laws that have considerable errors unless very large test specimens are used. Here we introduce a simple experimental method based on a higher-order quasi-brittle scaling law that has never been applied to snow nor any other geophysical material. We conducted hundreds of beam bending experiments using natural cohesive snow samples to produce the most comprehensive measurements to date of the tensile fracture toughness and effective process zone length of snow. We also adopt a new penetration resistance gauge to index the fracture toughness data, addressing a longstanding need for better proxy measurements to characterize snow structure. The peak penetration resistance met by a thin blade proved better than the bulk snow density for predicting fracture toughness, a finding that will improve field predictions and facilitate comparisons of results across studies. The tensile fracture process zone, previously a highly uncertain length scale related to avalanche fractures, is shown to be about 5-10 times the snow grain size, implying nonlinear fracture scaling for the majority of avalanches. C1 [Borstad, C. P.] Univ British Columbia, Dept Civil Engn, Vancouver, BC, Canada. [McClung, D. M.] Univ British Columbia, Dept Geog, Vancouver, BC, Canada. RP Borstad, CP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM cborstad@gmail.com OI Borstad, Christopher/0000-0001-6992-1770 FU Natural Sciences and Engineering Research Council of Canada; Canadian Mountain Holidays; University of British Columbia FX We are grateful for the financial support of the Natural Sciences and Engineering Research Council of Canada, Canadian Mountain Holidays, and the University of British Columbia. In-kind support was graciously provided by the Avalanche Control Section of Parks Canada at Rogers Pass. NR 50 TC 2 Z9 2 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD JUN PY 2013 VL 118 IS 2 BP 900 EP 912 DI 10.1002/jgrf.20065 PG 13 WC Geosciences, Multidisciplinary SC Geology GA 225VU UT WOS:000324993900035 ER PT J AU Nowicki, S Bindschadler, RA Abe-Ouchi, A Aschwanden, A Bueler, E Choi, H Fastook, J Granzow, G Greve, R Gutowski, G Herzfeld, U Jackson, C Johnson, J Khroulev, C Larour, E Levermann, A Lipscomb, WH Martin, MA Morlighem, M Parizek, BR Pollard, D Price, SF Ren, DD Rignot, E Saito, F Sato, T Seddik, H Seroussi, H Takahashi, K Walker, R Wang, WL AF Nowicki, Sophie Bindschadler, Robert A. Abe-Ouchi, Ayako Aschwanden, Andy Bueler, Ed Choi, Hyeungu Fastook, Jim Granzow, Glen Greve, Ralf Gutowski, Gail Herzfeld, Ute Jackson, Charles Johnson, Jesse Khroulev, Constantine Larour, Eric Levermann, Anders Lipscomb, William H. Martin, Maria A. Morlighem, Mathieu Parizek, Byron R. Pollard, David Price, Stephen F. Ren, Diandong Rignot, Eric Saito, Fuyuki Sato, Tatsuru Seddik, Hakime Seroussi, Helene Takahashi, Kunio Walker, Ryan Wang, Wei Li TI Insights into spatial sensitivities of ice mass response to environmental change from the SeaRISE ice sheet modeling project I: Antarctica SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article DE Antarctica; ice-sheet; sea-level; model; ensemble ID GROUNDING-LINE MIGRATION; INTERCOMPARISON PROJECT; OCEAN CIRCULATION; CLIMATE-CHANGE; SEA-LEVEL; PISM-PIK; PART 1; GREENLAND; SHELF; FLOW AB Atmospheric, oceanic, and subglacial forcing scenarios from the Sea-level Response to Ice Sheet Evolution (SeaRISE) project are applied to six three-dimensional thermomechanical ice-sheet models to assess Antarctic ice sheet sensitivity over a 500year timescale and to inform future modeling and field studies. Results indicate (i) growth with warming, except within low-latitude basins (where inland thickening is outpaced by marginal thinning); (ii) mass loss with enhanced sliding (with basins dominated by high driving stresses affected more than basins with low-surface-slope streaming ice); and (iii) mass loss with enhanced ice shelf melting (with changes in West Antarctica dominating the signal due to its marine setting and extensive ice shelves; cf. minimal impact in the Terre Adelie, George V, Oates, and Victoria Land region of East Antarctica). Ice loss due to dynamic changes associated with enhanced sliding and/or sub-shelf melting exceeds the gain due to increased precipitation. Furthermore, differences in results between and within basins as well as the controlling impact of sub-shelf melting on ice dynamics highlight the need for improved understanding of basal conditions, grounding-zone processes, ocean-ice interactions, and the numerical representation of all three. C1 [Nowicki, Sophie; Bindschadler, Robert A.; Walker, Ryan; Wang, Wei Li] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abe-Ouchi, Ayako] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba, Japan. [Aschwanden, Andy; Bueler, Ed; Khroulev, Constantine] Univ Alaska, Inst Geophys, Fairbanks, AR USA. [Choi, Hyeungu] Sigma Space Corp, Lanham, MD USA. [Fastook, Jim] Univ Maine, Comp Sci Quaternary Inst, Orono, ME USA. [Granzow, Glen; Johnson, Jesse] Univ Montana, Coll Arts & Sci, Missoula, MT 59812 USA. [Greve, Ralf; Sato, Tatsuru; Seddik, Hakime] Hokkaido Univ, Inst Low Temp Sci, Sapporo, Hokkaido 060, Japan. [Gutowski, Gail; Jackson, Charles] Univ Texas Austin, Inst Geophys, Austin, TX USA. [Herzfeld, Ute] Univ Colorado, Dept Elect Comp & Energy Engn, Boulder, CO 80309 USA. [Herzfeld, Ute] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Larour, Eric; Rignot, Eric; Seroussi, Helene] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Levermann, Anders; Martin, Maria A.] Potsdam Inst Climate Res, Potsdam, Germany. [Lipscomb, William H.; Price, Stephen F.] Los Alamos Natl Lab, Los Alamos, NM USA. [Morlighem, Mathieu; Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Parizek, Byron R.] Penn State DuBois, Math & Geosci, Du Bois, PA USA. [Pollard, David] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. [Ren, Diandong] Curtin Univ Technol, Dept Phys, Perth, WA, Australia. [Saito, Fuyuki; Takahashi, Kunio] Japan Agcy Marine Earth Sci & Technol, Res Inst Global Change, Kanazawa Ku, Yokohama, Kanagawa, Japan. [Walker, Ryan] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Nowicki, S (reprint author), NASA, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA. EM sophie.nowicki@nasa.gov RI Greve, Ralf/G-2336-2010; Abe-Ouchi, Ayako/M-6359-2013; Price, Stephen /E-1568-2013; Rignot, Eric/A-4560-2014; Seddik, Hakime/F-7640-2014; Morlighem, Mathieu/O-9942-2014; Jackson, Charles/A-2202-2009; Ren, Diandong/C-8870-2013; Levermann, Anders/G-4666-2011 OI SAITO, Fuyuki/0000-0001-5935-9614; Greve, Ralf/0000-0002-1341-4777; Abe-Ouchi, Ayako/0000-0003-1745-5952; Price, Stephen /0000-0001-6878-2553; Rignot, Eric/0000-0002-3366-0481; Seddik, Hakime/0000-0002-0241-590X; Morlighem, Mathieu/0000-0001-5219-1310; Jackson, Charles/0000-0002-2870-4494; Ren, Diandong/0000-0002-5757-7527; Levermann, Anders/0000-0003-4432-4704 FU Japan Society for the Promotion of Science (JSPS) [22244058]; NASA [NNX11AP39G, NNX-09-AV94G, NNX-10-AI04G, 281945.02.53.02.19]; German Federal Ministry of Education and Research (BMBF); U.S. National Science Foundation [0531211, 0758274, 0909335]; Center for Remote Sensing of Ice Sheets (CReSIS) [0424589]; US National Science Foundation [ANT-0424589, 1043018, 25-0550-0001, OCE-1202632]; U.S. Department of Energy (DOE) Office of Science Office of Biological and Environmental Research; DOE's Office of Science [DE-AC02-05CH11231, DE-AC05-00OR22725]; NASA Cryospheric Sciences Program; Jet Propulsion Laboratory Research Technology and Development Program; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center; NSF [0909335, CReSIS 0424589]; NASA Cryospheric Science program FX A project of this magnitude and scope required extensive support from many persons not listed as authors. Data sets, both published and in pre-publication forms, were contributed by A. LeBrocq, H. Pritchard, B. Csatho (dh/dt), T. Bracegirdle, CReSIS, and NASA's IceBridge mission and posted on the University of Montana CISM web site to be available to all SeaRISE modelers. This web site also served as a discussion forum for SeaRISE during its early stages of model initialization and experiment design. The Los Alamos National Laboratory also offered use of a web site that became the repository of all communication files (telecom notes and meeting presentations of SeaRISE). Participation in SeaRISE remained voluntary and, in most cases, came without financial support. Thus, participants had to leverage off of existing funding activities with objectives that overlapped with SeaRISE goals. [51] R. Greve, H. Seddik, and T. Sato were supported by a Grant-in-Aid for Scientific Research A (22244058) from the Japan Society for the Promotion of Science (JSPS). U. Herzfeld was supported by a NASA Cryospheric Sciences Award (NNX11AP39G). M. A. Martin was supported by the German Federal Ministry of Education and Research (BMBF). B. Parizek was supported by the U.S. National Science Foundation under grants 0531211, 0758274, 0909335, and the Center for Remote Sensing of Ice Sheets (CReSIS) 0424589 and by NASA under grants NNX-09-AV94G and NNX-10-AI04G. D. Pollard was supported by the US National Science Foundation under grants ANT-0424589, 1043018, 25-0550-0001, and OCE-1202632. S. F. Price and W. H. Lipscomb were supported by the U.S. Department of Energy (DOE) Office of Science Office of Biological and Environmental Research. Simulations were conducted at The National Energy Research Scientific Computing Center (supported by DOE's Office of Science under contract DE-AC02-05CH11231) using time awarded through DOE's ASCR Leadership Computing Challenge allocation to the project "Projections of Ice Sheet Evolution Using Advanced Ice and Ocean Models." Model development and simulations were also conducted at the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, supported by DOE's Office of Science under contract DE-AC05-00OR22725. CISM development and simulations relied on additional support by K. J. Evans, P. H. Worley, and J. A. Nichols (all of Oak Ridge National Laboratory) and by A. G. Salinger (Sandia National Laboratories). H. Seroussi and M. Morlighem are supported by the NASA Cryospheric Sciences Program and Modeling Analysis and Prediction Program and a contract with the Jet Propulsion Laboratory Research Technology and Development Program. H. Seroussi was also supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. E. Larour and E. Rignot further enabled their participation on SeaRISE. R. Walker was supported by NSF through grants 0909335 and CReSIS 0424589, by NASA under grants NNX-09-AV94G and NNX-10-AI04G, and by the Gary Comer Science and Education Foundation. W. Wang was supported by the NASA Cryospheric Science program (grant 281945.02.53.02.19). Finally, S. Nowicki and R.; Bindschadler wish to gratefully acknowledge the unwavering encouragement and financial support from the NASA Cryospheric Science program for the core funding enabling SeaRISE to reach a successful conclusion. We thank the reviewers (two anonymous and A. Vieli), the Associate Editor P. Christoffersen, and the Editor B. Hubbard for their very thoughtful comments to the original draft that led to a more constructive final manuscript. NR 119 TC 20 Z9 20 U1 0 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD JUN PY 2013 VL 118 IS 2 BP 1002 EP 1024 DI 10.1002/jgrf.20081 PG 23 WC Geosciences, Multidisciplinary SC Geology GA 225VU UT WOS:000324993900042 ER PT J AU Nowicki, S Bindschadler, RA Abe-Ouchi, A Aschwanden, A Bueler, E Choi, H Fastook, J Granzow, G Greve, R Gutowski, G Herzfeld, U Jackson, C Johnson, J Khroulev, C Larour, E Levermann, A Lipscomb, WH Martin, MA Morlighem, M Parizek, BR Pollard, D Price, SF Ren, DD Rignot, E Saito, F Sato, T Seddik, H Seroussi, H Takahashi, K Walker, R Wang, WL AF Nowicki, Sophie Bindschadler, Robert A. Abe-Ouchi, Ayako Aschwanden, Andy Bueler, Ed Choi, Hyeungu Fastook, Jim Granzow, Glen Greve, Ralf Gutowski, Gail Herzfeld, Ute Jackson, Charles Johnson, Jesse Khroulev, Constantine Larour, Eric Levermann, Anders Lipscomb, William H. Martin, Maria A. Morlighem, Mathieu Parizek, Byron R. Pollard, David Price, Stephen F. Ren, Diandong Rignot, Eric Saito, Fuyuki Sato, Tatsuru Seddik, Hakime Seroussi, Helene Takahashi, Kunio Walker, Ryan Wang, Wei Li TI Insights into spatial sensitivities of ice mass response to environmental change from the SeaRISE ice sheet modeling project II: Greenland SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article DE Greenland; ice-sheet; sea-level; model; ensemble ID OUTLET GLACIER; CLIMATE-CHANGE; SURFACE MELT; SEA-LEVEL; ANTARCTICA; ACCELERATION; FLOW; SIMULATIONS; VARIABILITY; BALANCE AB The Sea-level Response to Ice Sheet Evolution (SeaRISE) effort explores the sensitivity of the current generation of ice sheet models to external forcing to gain insight into the potential future contribution to sea level from the Greenland and Antarctic ice sheets. All participating models simulated the ice sheet response to three types of external forcings: a change in oceanic condition, a warmer atmospheric environment, and enhanced basal lubrication. Here an analysis of the spatial response of the Greenland ice sheet is presented, and the impact of model physics and spin-up on the projections is explored. Although the modeled responses are not always homogeneous, consistent spatial trends emerge from the ensemble analysis, indicating distinct vulnerabilities of the Greenland ice sheet. There are clear response patterns associated with each forcing, and a similar mass loss at the full ice sheet scale will result in different mass losses at the regional scale, as well as distinct thickness changes over the ice sheet. All forcings lead to an increased mass loss for the coming centuries, with increased basal lubrication and warmer ocean conditions affecting mainly outlet glaciers, while the impacts of atmospheric forcings affect the whole ice sheet. C1 [Nowicki, Sophie; Bindschadler, Robert A.; Walker, Ryan; Wang, Wei Li] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abe-Ouchi, Ayako] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba, Japan. [Aschwanden, Andy; Bueler, Ed; Khroulev, Constantine] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Choi, Hyeungu] Sigma Space Corp, Lanham, MD USA. [Fastook, Jim] Univ Maine, Comp Sci Quaternary Inst, Orono, ME USA. [Granzow, Glen; Johnson, Jesse] Univ Montana, Coll Arts & Sci, Missoula, MT 59812 USA. [Greve, Ralf; Sato, Tatsuru; Seddik, Hakime] Hokkaido Univ, Inst Low Temp Sci, Sapporo, Hokkaido 060, Japan. [Gutowski, Gail; Jackson, Charles] Univ Texas Austin, Inst Geophys, Austin, TX USA. [Herzfeld, Ute] Univ Colorado, Dept Elect Comp & Energy Engn, Boulder, CO 80309 USA. [Herzfeld, Ute] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Larour, Eric; Rignot, Eric; Seroussi, Helene] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Levermann, Anders; Martin, Maria A.] Univ Potsdam, Inst Phys, Potsdam, Germany. [Lipscomb, William H.; Price, Stephen F.] Los Alamos Natl Lab, Los Alamos, NM USA. [Morlighem, Mathieu; Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Parizek, Byron R.] Penn State DuBois, Dept Math & Geosci, Du Bois, PA USA. [Pollard, David] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. [Ren, Diandong] Curtin Univ Technol, Dept Phys, Perth, WA, Australia. [Saito, Fuyuki; Takahashi, Kunio] Japan Agcy Marine Earth Sci & Technol, Res Inst Global Change, Yokohama, Kanagawa, Japan. [Walker, Ryan] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Nowicki, S (reprint author), NASA, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA. EM sophie.nowicki@nasa.gov RI Greve, Ralf/G-2336-2010; Abe-Ouchi, Ayako/M-6359-2013; Price, Stephen /E-1568-2013; Rignot, Eric/A-4560-2014; Seddik, Hakime/F-7640-2014; Morlighem, Mathieu/O-9942-2014; Jackson, Charles/A-2202-2009; Ren, Diandong/C-8870-2013; Levermann, Anders/G-4666-2011; OI Greve, Ralf/0000-0002-1341-4777; Abe-Ouchi, Ayako/0000-0003-1745-5952; Price, Stephen /0000-0001-6878-2553; Rignot, Eric/0000-0002-3366-0481; Seddik, Hakime/0000-0002-0241-590X; Morlighem, Mathieu/0000-0001-5219-1310; Jackson, Charles/0000-0002-2870-4494; Ren, Diandong/0000-0002-5757-7527; Levermann, Anders/0000-0003-4432-4704; SAITO, Fuyuki/0000-0001-5935-9614 FU Japan Society for the Promotion of Science (JSPS) [22244058]; NASA Cryospheric Sciences Award [NNX11AP39G]; German Federal Ministry of Education and Research (BMBF); U.S. National Science Foundation [0531211, 0758274, 0909335, ANT-0424589, 1043018, 25-0550-0001, OCE-1202632]; Center for Remote Sensing of Ice Sheets (CReSIS) [0424589]; NASA [NNX-09-AV94G, NNX-10-AI04G]; U.S. Department of Energy (DOE) Office of Science, Biological and Environmental Research; DOE's Office of Science [DE-AC02-05CH11231, DE-AC05-00OR22725]; DOE's ASCR; NASA Postdoctoral Program at the Jet Propulsion Laboratory; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center; NSF [0909335, CReSIS 0424589]; Gary Comer Science and Education Foundation; NASA Cryospheric Science program [281945.02.53.02.19]; NASA Cryospheric Science program FX R. Greve, H. Seddik, and T. Sato were supported by a Grant-in-Aid for Scientific Research (22244058) from the Japan Society for the Promotion of Science (JSPS). U. Herzfeld was supported by a NASA Cryospheric Sciences Award (NNX11AP39G). M. A. Martin was supported by the German Federal Ministry of Education and Research (BMBF). B. Parizek was supported by the U.S. National Science Foundation under grants 0531211, 0758274, 0909335 and the Center for Remote Sensing of Ice Sheets (CReSIS) 0424589, and by NASA under grants NNX-09-AV94G and NNX-10-AI04G. D. Pollard was supported by the U.S. National Science Foundation under grants ANT-0424589, 1043018, 25-0550-0001, and OCE-1202632. S. F. Price and W. H. Lipscomb were supported by the U.S. Department of Energy (DOE) Office of Science, Biological and Environmental Research. Simulations were conducted at the National Energy Research Scientific Computing Center (supported by DOE's Office of Science under contract DE-AC02-05CH11231) using time awarded through DOE's ASCR Leadership Computing Challenge allocation to the project "Projections of Ice Sheet Evolution Using Advanced Ice and Ocean Models." Model development and simulations were also conducted at the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, supported by DOE's Office of Science under contract DE-AC05-00OR22725. CISM development and simulations relied on additional support by K.J. Evans, P. H. Worley, and J.A. Nichols (all of Oak Ridge National Laboratory) and A. G. Salinger (Sandia National Laboratories). H Seroussi and M. Morlighem are supported by the NASA Cryospheric Sciences Program and Modeling Analysis and Prediction Program and a contract with the Jet Propulsion Laboratory Research Technology and Development Program. H Seroussi was also supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. E. Larour and E. Rignot further enabled their participation on SeaRISE. R. Walker was supported by NSF through grants 0909335 and CReSIS 0424589, by NASA under grants NNX-09-AV94G and NNX-10-AI04G, and by the Gary Comer Science and Education Foundation. W. Wang was supported by the NASA Cryospheric Science program (grant 281945.02.53.02.19). Finally, S. Nowicki and R. Bindschadler wish to gratefully acknowledge the unwavering encouragement and financial support from the NASA Cryospheric Science program for the core funding enabling SeaRISE to reach a successful conclusion. We thank the reviewers (one anonymous and A. Vieli) and the Associate Editor P. Christoffersen for their very thoughtful comments to the original draft that led to a more constructive final manuscript. NR 84 TC 31 Z9 31 U1 3 U2 37 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD JUN PY 2013 VL 118 IS 2 BP 1025 EP 1044 DI 10.1002/jgrf.20076 PG 20 WC Geosciences, Multidisciplinary SC Geology GA 225VU UT WOS:000324993900043 ER PT J AU Kirchner, N Furrer, R Jakobsson, M Zwally, HJ Robbins, JW AF Kirchner, N. Furrer, R. Jakobsson, M. Zwally, H. J. Robbins, J. W. TI Statistical modeling of a former Arctic Ocean ice shelf complex using Antarctic analogies SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article DE Arctic Ocean ice shelves; extreme value theory; deep-draft ice berg scours; multivariate linear model; ICESat data in Arctic-Antarctic analogy approach ID LAST GLACIAL MAXIMUM; LOMONOSOV RIDGE; YERMAK PLATEAU; MARINE-ICE; SHEET; SEA; SEDIMENTATION; SENSITIVITY; LAURENTIDE; ICEBERGS AB Geophysical mapping and coring of the central Arctic Ocean seafloor provide evidence for repeated occurrences of ice sheet/ice shelf complexes during previous glacial periods. Several ridges and bathymetric highs shallower than present water depths of approximate to 1000m show signs of erosion from deep-drafting (armadas of) icebergs, which originated from thick outlet glaciers and ice shelves. Mapped glacigenic landforms and dates of cored sediments suggest that the largest ice shelf complex was confined to the Amerasian sector of the Arctic Ocean during Marine Isotope Stage (MIS) 6. However, the spatial extent of ice shelves can not be well reconstructed from occasional groundings on bathymetric highs. Therefore, we apply a statistical approach to provide independent support for an extensive MIS 6 ice shelf complex, which previously was inferred only from interpretation of geophysical and geological data. Specifically, we assess whether this ice shelf complex comprises a likely source of the deep-draft icebergs responsible for the mapped scour marks. The statistical modeling is based on exploiting relations between contemporary Antarctic ice shelves and their local physical environments and the assumption that Arctic Ocean MIS6 ice shelves scale similarly. Analyzing ice thickness data along the calving front of contemporary ice shelves, a peak over threshold method is applied to determine sources of deep-drafting icebergs in the Arctic Ocean MIS6 ice shelf complex. This approach is novel to modeling Arctic paleoglacial configurations. Predicted extreme calving front drafts match observed deep-draft iceberg scours if the ice shelf complex is sufficiently large. C1 [Kirchner, N.] Stockholm Univ, Dept Phys Geog & Quaternary Geol, S-10691 Stockholm, Sweden. [Furrer, R.] Univ Zurich, Inst Math, CH-8001 Zurich, Switzerland. [Jakobsson, M.] Stockholm Univ, Dept Geol Sci, S-10691 Stockholm, Sweden. [Zwally, H. J.; Robbins, J. W.] NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Kirchner, N (reprint author), Stockholm Univ, Dept Phys Geog & Quaternary Geol, S-10691 Stockholm, Sweden. EM nina.kirchner@natgeo.su.se RI Furrer, Reinhard/A-4580-2011; Jakobsson, Martin/F-6214-2010; OI Furrer, Reinhard/0000-0002-6319-2332; Jakobsson, Martin/0000-0002-9033-3559 FU SNSF [129782, 143282]; URPP Systems Biology FX N.K. and R. F. are joint first authors of this manuscript. N.K. thanks C. Stover Wiederwohl, Texas A&M University, for introduction to and guidance through the WOCE-SODB database during the "Oden Southern Ocean 0910" cruise to Pine Island Bay/West Antarctica. R. F. acknowledges funding from SNSF 129782, 143282 and URPP Systems Biology. This is a contribution from the Bolin Center for Climate Research at Stockholm University, Sweden. We thank the editor, Bryn Hubbard, the associate editor, Mike Bentley, as well as Jesse Johnson, and five anonymous reviewers for valuable comments on the manuscript. NR 47 TC 1 Z9 1 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD JUN PY 2013 VL 118 IS 2 BP 1105 EP 1117 DI 10.1002/jgrf.20077 PG 13 WC Geosciences, Multidisciplinary SC Geology GA 225VU UT WOS:000324993900047 ER PT J AU Brucker, L Markus, T AF Brucker, Ludovic Markus, Thorsten TI Arctic-scale assessment of satellite passive microwave-derived snow depth on sea ice using Operation IceBridge airborne data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE SD on sea ice; evaluation of satellite product; Operation IceBridge Airborne data ID AMSR-E; RADAR BACKSCATTER; RETRIEVALS; ROUGHNESS; EXCHANGE; ENERGY; EOS AB Snow depth on sea ice (SD) is a key geophysical variable, knowledge of which is critical for calculating the energy and mass balance budgets. Moreover, accurate knowledge of the SD distribution is important to retrieve sea-ice thicknesses from altimetry data. So far, only space-based microwave radiometers (e.g., Advanced Microwave Scanning Radiometer for Earth Observing System; AMSR-E) provide operational SD on seasonal sea-ice retrievals. A thorough assessment of these retrievals is needed on a large scale and on a variety of sea-ice types. Our study presents such an assessment on Arctic sea ice using NASA's airborne Operation IceBridge (OIB) SDs, retrieved from radar measurements. Between 2009 and 2011, approximate to 610 12.5 km satellite grid cells were covered by seasonal sea ice where both satellite SD retrievals and OIB data were available. Using all the available data, the difference between the AMSR-E product and the averaged OIB snow-radar-derived SD is 0.000.07 m. Satellite-derived SD was accurate in the Beaufort Sea and the Canadian Archipelago but underestimated (approximate to 0.07 m) in the Nares Strait. The RMSE between the two products ranges between 0.03 and 0.15 m. The RMSE is less than 0.06 m over a shallow snow cover (<0.20 m), in areas where satellite-retrieved ice concentrations are higher than 90%, surface smooth, and ice thicker than approximate to 0.5 m. Locally the AMSR-E algorithm can significantly underestimate SD. Several regions where the retrievals were less accurate (error >0.10 m) have been identified and related to the presence of either low ice concentration or significant fraction of multiyear ice within the grid cell that has not been flagged. C1 [Brucker, Ludovic; Markus, Thorsten] NASA GSFC, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Brucker, Ludovic] Univ Space Res Assoc, Greenbelt, MD USA. RP Brucker, L (reprint author), NASA GSFC, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA. EM ludovic.brucker@nasa.gov RI Brucker, Ludovic/A-8029-2010 OI Brucker, Ludovic/0000-0001-7102-8084 NR 25 TC 14 Z9 14 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD JUN PY 2013 VL 118 IS 6 BP 2892 EP 2905 DI 10.1002/jgrc.20228 PG 14 WC Oceanography SC Oceanography GA 224KZ UT WOS:000324885500010 ER PT J AU Hauck, SA Margot, JL Solomon, SC Phillips, RJ Johnson, CL Lemoine, FG Mazarico, E McCoy, TJ Padovan, S Peale, SJ Perry, ME Smith, DE Zuber, MT AF Hauck, Steven A., II Margot, Jean-Luc Solomon, Sean C. Phillips, Roger J. Johnson, Catherine L. Lemoine, Frank G. Mazarico, Erwan McCoy, Timothy J. Padovan, Sebastiano Peale, Stanton J. Perry, Mark E. Smith, David E. Zuber, Maria T. TI The curious case of Mercury's internal structure SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mercury; Internal Structure; MESSENGER ID EQUATION-OF-STATE; FE-RICH PORTION; HIGH-PRESSURE; MAGNETIC-FIELD; GRAVITY-FIELD; EARTHS CORE; MELTING RELATIONS; HIGH-TEMPERATURE; PLANETARY CORES; PHASE-RELATIONS AB The recent determination of the gravity field of Mercury and new Earth-based radar observations of the planet's spin state afford the opportunity to explore Mercury's internal structure. These observations provide estimates of two measures of the radial mass distribution of Mercury: the normalized polar moment of inertia and the fractional polar moment of inertia of the solid portion of the planet overlying the liquid core. Employing Monte Carlo techniques, we calculate several million models of the radial density structure of Mercury consistent with its radius and bulk density and constrained by these moment of inertia parameters. We estimate that the top of the liquid core is at a radius of 202030km, the mean density above this boundary is 3380200kgm(-3), and the density below the boundary is 6980280kgm(-3). We find that these internal structure parameters are robust across a broad range of compositional models for the core and planet as a whole. Geochemical observations of Mercury's surface by MESSENGER indicate a chemically reducing environment that would favor the partitioning of silicon or both silicon and sulfur into the metallic core during core-mantle differentiation. For a core composed of Fe-S-Si materials, the thermodynamic properties at elevated pressures and temperatures suggest that an FeS-rich layer could form at the top of the core and that a portion of it may be presently solid. C1 [Hauck, Steven A., II] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. [Margot, Jean-Luc] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Margot, Jean-Luc; Padovan, Sebastiano] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO USA. [Johnson, Catherine L.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada. [Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ USA. [Lemoine, Frank G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mazarico, Erwan; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. [Peale, Stanton J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Perry, Mark E.] Johns Hopkins Appl Phys Lab, Space Dept, Laurel, MD USA. RP Hauck, SA (reprint author), Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. EM hauck@case.edu RI Hauck, Steven/A-7865-2008; Margot, Jean-Luc/A-6154-2012; Lemoine, Frank/D-1215-2013; Mazarico, Erwan/N-6034-2014; Perry, Mark/B-8870-2016 OI Hauck, Steven/0000-0001-8245-146X; Margot, Jean-Luc/0000-0001-9798-1797; Mazarico, Erwan/0000-0003-3456-427X; Perry, Mark/0000-0003-1600-6856 FU NASA MESSENGER [NNX07AR77G]; NASA [NASW-00002, NAS5-97271] FX We thank the entire MESSENGER team for the development and operation of the mission and the acquisition of the data from the first spacecraft to orbit Mercury. Discussions with Larry Nittler and Nathalie Michel on an early draft are greatly appreciated. Comments by Frank Sohl and an anonymous reviewer helped sharpen the manuscript. This work is supported by NASA MESSENGER Participating Scientist grant NNX07AR77G to S. A. H. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory. This work made use of the High Performance Computing Resource in the Core Facility for Advanced Research Computing at Case Western Reserve University. NR 73 TC 52 Z9 52 U1 3 U2 40 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN PY 2013 VL 118 IS 6 BP 1204 EP 1220 DI 10.1002/jgre.20091 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TI UT WOS:000324911900004 ER PT J AU Thomson, BJ Bridges, NT Cohen, J Hurowitz, JA Lennon, A Paulsen, G Zacny, K AF Thomson, B. J. Bridges, N. T. Cohen, J. Hurowitz, J. A. Lennon, A. Paulsen, G. Zacny, K. TI Estimating rock compressive strength from Rock Abrasion Tool (RAT) grinds SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; physical properties; basalt; rock strength; MER ID GUSEV CRATER; SANDSTONE AB Each Mars Exploration Rover carries a Rock Abrasion Tool (RAT) whose intended use was to abrade the outer surfaces of rocks to expose more pristine material. Motor currents drawn by the RAT motors are related to the strength and hardness of rock surfaces undergoing abrasion, and these data can be used to infer more about a target rock's physical properties. However, no calibration of the RAT exists. Here, we attempt to derive an empirical correlation using an assemblage of terrestrial rocks and apply this correlation to data returned by the rover Spirit. The results demonstrate a positive correlation between rock strength and RAT grind energy for rocks with compressive strengths less than about 150MPa, a category that includes all but the strongest intact rocks. Applying this correlation to rocks abraded by Spirit's RAT, the results indicate a large divide in strength between more competent basaltic rocks encountered in the plains of Gusev crater (Adirondack-class rocks) and the weaker variety of rock types measured in the Columbia Hills. Adirondack-class rocks have estimated compressive strengths in the range of 70-130MPa and are significantly less strong than fresh terrestrial basalts; this may be indicative of a degree of weathering-induced weakening. Rock types in the Columbia Hills (Wishstone, Watchtower, Clovis, and Peace class) all have compressive strengths <50MPa and are consistent with impactites or volcanoclastic materials. In general, when considered alongside chemical, spectral, and rock textural data, these inferred compressive strength results help inform our understanding of rock origins and modification history. C1 [Thomson, B. J.] Boston Univ, Ctr Remote Sensing, Boston, MA 02215 USA. [Bridges, N. T.; Lennon, A.] Johns Hopkins Appl Phys Lab, Laurel, MD USA. [Cohen, J.; Paulsen, G.; Zacny, K.] Honeybee Robot, Pasadena, CA USA. [Hurowitz, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Thomson, BJ (reprint author), Boston Univ, Ctr Remote Sensing, 725 Commonwealth Ave,Rm 433, Boston, MA 02215 USA. EM bjt@bu.edu RI Bridges, Nathan/D-6341-2016 FU NASA FX This project has benefitted from helpful discussions with current and former Honeybee Robotics engineers; insightful and constructive reviews from Ralph Lorenz and an anonymous reviewer also improved the manuscript. Support for this research was provided by a NASA Mars Fundamental Research Program grant to BJT. The authors also gratefully acknowledge Robert Anderson and Gregory Peters from JPL for help with rock sample procurement. NR 36 TC 5 Z9 5 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN PY 2013 VL 118 IS 6 BP 1233 EP 1244 DI 10.1002/jgre.20061 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TI UT WOS:000324911900006 ER PT J AU Jordan, AP Stubbs, TJ Joyce, CJ Schwadron, NA Spence, HE Wilson, JK AF Jordan, A. P. Stubbs, T. J. Joyce, C. J. Schwadron, N. A. Spence, H. E. Wilson, J. K. TI The formation of molecular hydrogen from water ice in the lunar regolith by energetic charged particles SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE galactic cosmic rays; solar energetic particles; water ice; permanently shadowed region; Moon; molecular hydrogen ID SOLAR-WIND; UV PHOTOLYSIS; BOMBARDMENT; IRRADIATION; POLES; RADIATION; DEPOSITS; RECORD; PLUME; MOON AB On 9 October 2009, the Lunar Crater Observation and Sensing Satellite (LCROSS) mission impacted a spent Centaur rocket into the permanently shadowed region (PSR) within Cabeus crater and detected water vapor and ice, as well as other volatiles, in the ejecta plume. The Lyman Alpha Mapping Project (LAMP), a far ultraviolet (FUV) imaging spectrograph on board the Lunar Reconnaissance Orbiter (LRO), observed this plume as FUV emissions from the fluorescence of sunlight by molecular hydrogen (H-2) and other constituents. Energetic charged particles, such as galactic cosmic rays (GCRs) and solar energetic particles (SEPs), can dissociate the molecules in water ice to form H-2. We examine how much H(2)can be formed by these types of particle radiation interacting with water ice sequestered in the regolith within PSRs, and we assess whether it can account for the H-2 observed by LAMP. To estimate H(2)formation, we use the GCR and SEP radiation dose rates measured by the LRO Cosmic Ray Telescope for the Effects of Radiation (CRaTER). The exposure time of the ice is calculated by considering meteoritic gardening and the penetration depth of the energetic particles. We find that GCRs and SEPs could convert at least 1-7% of the original water molecules into H-2. Therefore, given the amount of water detected by LCROSS, such particle radiationinduced dissociation of water ice could likely account for a significant percentage (10-100%) of the H(2)measured by LAMP. C1 [Jordan, A. P.; Joyce, C. J.; Schwadron, N. A.; Spence, H. E.; Wilson, J. K.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Stubbs, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Jordan, AP (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Morse Hall Room 308,8 Coll Rd, Durham, NH 03824 USA. EM a.p.jordan@unh.edu RI Stubbs, Timothy/I-5139-2013; OI Stubbs, Timothy/0000-0002-5524-645X; Spence, Harlan/0000-0002-2526-2205 FU NASA [NNG11PA03C] FX This work was supported by NASA grant NNG11PA03C. The authors wish to thank Alex Crew and Alex Boyd for helpful discussions. The authors also wish to thank the two reviewers for their valuable suggestions for improving this paper. The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. NR 52 TC 9 Z9 9 U1 2 U2 11 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 JUN PY 2013 VL 118 IS 6 BP 1257 EP 1264 DI 10.1002/jgre.20095 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TI UT WOS:000324911900008 ER PT J AU Kahre, MA Vines, SK Haberle, RM Hollingsworth, JL AF Kahre, Melinda A. Vines, Sarah K. Haberle, Robert M. Hollingsworth, Jeffery L. TI The early Martian atmosphere: Investigating the role of the dust cycle in the possible maintenance of two stable climate states SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; atmosphere ID GENERAL-CIRCULATION MODEL; PARTICLE SIZES; MARS; SIMULATIONS AB C. Leovy (personal communication, 2007) speculated that two stable climate states on early Mars could have resulted from interactions between the dust and CO2 cycles. In one state, a highly active dust cycle would prevent atmospheric collapse, and in the second, the collapsed atmosphere would not maintain an active dust cycle. An initial assessment of this idea is presented based on a Mars general circulation model parameter study. A range of global dust loadings, CO2 ice albedos, and obliquities are investigated to explore conditions in which increasing the atmospheric dust content stabilizes an otherwise unstable atmosphere. We find that dust only stabilizes the atmosphere at high obliquity and when the CO2 ice albedo is high. Although results suggest that two stable states could have existed on early Mars under limited conditions, further work is needed to know if the conditions necessary are physically plausible. C1 [Kahre, Melinda A.; Haberle, Robert M.; Hollingsworth, Jeffery L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Vines, Sarah K.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA. RP Kahre, MA (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM melinda.a.kahre@nasa.gov RI Dennis, Allison/A-7654-2014 FU Mars Fundamental Research Program FX This project would not have come about if it were not for Conway Leovy. His participation in this ongoing work will be greatly missed. This work was funded by the Mars Fundamental Research Program. The authors thank Claire Newman and an anonymous reviewer for their insightful comments and suggestions. NR 31 TC 5 Z9 5 U1 2 U2 6 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 JUN PY 2013 VL 118 IS 6 BP 1388 EP 1396 DI 10.1002/jgre.20099 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TI UT WOS:000324911900015 ER PT J AU Matteini, L Hellinger, P Goldstein, BE Landi, S Velli, M Neugebauer, M AF Matteini, Lorenzo Hellinger, Petr Goldstein, Bruce E. Landi, Simone Velli, Marco Neugebauer, Marcia TI Signatures of kinetic instabilities in the solar wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Solar Wind; Kinetic Instabilities; Observations in situ; Space Plasmas ID ELECTROMAGNETIC PROTON/PROTON INSTABILITIES; PROTON TEMPERATURE ANISOTROPY; ULYSSES OBSERVATIONS; ION-BEAMS; PLASMA; VELOCITY; DISTRIBUTIONS; CONSTRAINT; COLLISIONS; TURBULENCE AB An analysis of ion non-thermal properties in the fast solar wind based on Ulysses data is reported. The radial evolution of the main proton moments (density, temperature, and drift velocities) and their empirical correlations with other plasma parameters are investigated in detail and compared with theoretical expectations. The stability of the plasma is studied against different ion kinetic instabilities driven by ion temperature anisotropies and differential velocities, focusing on the identification of possible signatures of relevant instabilities in the observed core-beam structure of proton distributions. The temperature anisotropy of the total proton distribution appears to be constrained by fire hose instabilities, in agreement with previous studies, while if considered separately, beam and core populations exhibit opposite anisotropies, with core protons characterized by perpendicular temperatures larger than the parallel ones, possibly (marginally) unstable for ion-cyclotron instability. The evolution with distance of the drift velocity between the secondary population and the main core is found to be nonadiabatic, leading to the identification of a marginal stability path of a magnetosonic ion-beam instability. As a conclusion, we find that a large fraction of the proton distributions observed by Ulysses display signatures of either a beam or a fire hose instability, suggesting that such kinetic processes play an important role in regulating the solar wind thermal energetics during the plasma expansion. C1 [Matteini, Lorenzo] Univ London Imperial Coll Sci Technol & Med, Dept Phys, Blackett Lab, London SW7 2AZ, England. [Matteini, Lorenzo; Landi, Simone; Velli, Marco] Univ Florence, Dipartimento Fis & Astron, Florence, Italy. [Hellinger, Petr] AS CR, Astron Inst, Prague, Czech Republic. [Goldstein, Bruce E.; Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Neugebauer, Marcia] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Matteini, L (reprint author), Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England. EM matteini@arcetri.astro.it RI Hellinger, Petr/F-5267-2014; Landi, Simone/G-7282-2015 OI Hellinger, Petr/0000-0002-5608-0834; Landi, Simone/0000-0002-1322-8712 FU European Commission [284515]; Science and Technology Facilities Council (STFC); Grant Agency of the Czech Republic [P209/12/2023]; National Aeronautics and Space Administration FX The authors thank Roland Grappin, Tim Horbury, and Robert Wicks for useful discussions. The research leading to these results has received funding from the European Commission's Seventh Framework Programme (FP7) under the grant agreement SHOCK (project 284515) and from the Science and Technology Facilities Council (STFC). PH acknowledges the grant P209/12/2023 of the Grant Agency of the Czech Republic. The research described in this paper was also carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 54 TC 28 Z9 28 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 2771 EP 2782 DI 10.1002/jgra.50320 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100002 ER PT J AU Le, G Chi, PJ Blanco-Cano, X Boardsen, S Slavin, JA Anderson, BJ Korth, H AF Le, Guan Chi, Peter J. Blanco-Cano, Xochitl Boardsen, Scott Slavin, James A. Anderson, Brian J. Korth, Haje TI Upstream ultra-low frequency waves in Mercury's foreshock region: MESSENGER magnetic field observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Mercury upstream waves; Mercury's foreshock; MESSENGER spacecraft; Low Mach number shocks; Upstream whistler waves; Upstream magnetosonic waves ID EARTHS BOW SHOCK; ONE-HERTZ WAVES; COLLISIONLESS SHOCKS; IONS UPSTREAM; MACH-NUMBER; ULF WAVES; MAGNETOSHEATH; BEAMS; ACCELERATION; BOUNDARY AB Mercury's bow shock is unique in our solar system as it is produced by low Mach number solar wind blowing over a small magnetized body. The availability of MESSENGER orbiter data enables us for the first time to conduct an in-depth study of upstream waves in Mercury's foreshock. This paper reports first results of an observational study of upstream ULF waves in Mercury's foreshock using high-time resolution magnetic field data from the MESSENGER spacecraft to understand the general morphology of these waves. We find that the most common wave phenomenon in Mercury's foreshock has frequencies2Hz, with properties similar to the 1 Hz whistler waves in the Earth's foreshock. Their generation appears to be generic to the shock and not affected by the weak strength and small size of Mercury's bow shock. On the other hand, the most common wave phenomenon in the Earth's foreshock is the large-amplitude 30 second waves, identified as fast magnetosonic waves generated by backstreaming ions. Similar waves at Mercury have wave frequencies at0.3Hz, but occur only sporadically. The general lack of strong 30 second magnetosonic waves at Mercury can be attributed to the lack of strong backstreaming ions due to a weak bow shock and not enough time for wave growth due to the small foreshock size. Superposed on the 1 Hz whistler waves, there are short bursts of spectral peaks at0.8Hz that are new and have not been reported previously in Mariner 10 data. C1 [Le, Guan; Chi, Peter J.; Boardsen, Scott] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Space Weather Lab, Greenbelt, MD 20771 USA. [Chi, Peter J.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Blanco-Cano, Xochitl] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City, DF, Mexico. [Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Le, G (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA. EM Guan.Le@nasa.gov RI Slavin, James/H-3170-2012; Le, Guan/C-9524-2012 OI Slavin, James/0000-0002-9206-724X; Le, Guan/0000-0002-9504-5214 NR 52 TC 12 Z9 12 U1 2 U2 12 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 JUN PY 2013 VL 118 IS 6 BP 2809 EP 2823 DI 10.1002/jgra.50342 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100006 ER PT J AU Maneva, YG Vinas, AF Ofman, L AF Maneva, Y. G. Vinas, A. F. Ofman, L. TI Turbulent heating and acceleration of He++ ions by spectra of Alfven-cyclotron waves in the expanding solar wind: 1.5-D hybrid simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE turbulent heating; ion acceleration; solar wind expansion; Alfven-cyclotron waves; wave-particle interactions; parametric decays ID DIFFERENTIAL FLOW; PLASMA; CORONA; DISTRIBUTIONS; ANISOTROPIES; PARTICLE; PROTONS; ULYSSES AB Both remote sensing and in situ measurements show that the fast solar wind plasma significantly deviates from thermal equilibrium and is strongly permeated by turbulent electromagnetic waves, which regulate the ion temperature anisotropies and relative drifts. Thus, the ion kinetics is governed by heating and cooling related to absorption and emission of ion-acoustic and ion-cyclotron waves, as well as nonresonant pitch angle scattering and diffusion in phase space. Additionally, the solar wind properties are affected by its nonadiabatic expansion as the wind travels away from the Sun. In this study we present results from 1.5-D hybrid simulations to investigate the effects of a nonlinear turbulent spectrum of Alfven-cyclotron waves and the solar wind expansion on the anisotropic heating and differential acceleration of protons and He++ ions. We compare the different heating and acceleration by turbulent Alfven-cyclotron wave spectra and by pure monochromatic waves. For the waves and the wave spectra used in our model, we find that the He++ ions are preferentially heated and by the end of the simulations acquire much more than mass-proportional temperature ratios, T/T-p>m/m(p). The differential acceleration between the two species strongly depends on the initial wave amplitude and the related spectral index and is often suppressed by the solar wind expansion. We also find that the expansion leads to perpendicular cooling for both species, and depending on the initial wave spectra, it can either heat or cool the ions in parallel direction. Despite the cooling effect of the expansion in perpendicular direction, the wave-particle interactions provide an additional heating source, and the perpendicular temperature components remain higher than the adiabatic predictions. C1 [Maneva, Y. G.; Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Maneva, Y. G.; Vinas, A. F.; Ofman, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Maneva, YG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM yana.g.maneva@nasa.gov FU NASA [NNX10AC56G] FX This work was supported by NASA, grant NNX10AC56G. The 1.5-D code used to obtain the results of this paper is an extension of the hybrid code used by Araneda et al. [2009]. Fruitful discussions with J. Araneda are highly appreciated. NR 38 TC 18 Z9 18 U1 0 U2 2 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 JUN PY 2013 VL 118 IS 6 BP 2842 EP 2853 DI 10.1002/jgra.50363 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100009 ER PT J AU Jones, SL Lessard, MR Rychert, K Spanswick, E Donovan, E Jaynes, AN AF Jones, S. L. Lessard, M. R. Rychert, K. Spanswick, E. Donovan, E. Jaynes, A. N. TI Persistent, widespread pulsating aurora: A case study SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE pulsating aurora; substorm onset; recovery phase ID PITCH-ANGLE DIFFUSION; MORNINGSIDE AURORAE; FAST SATELLITE; MORPHOLOGY; OBSERVATORIES; GENERATION; SUBSTORMS; EXPANSION; ELECTRONS; REGION AB Observations of a pulsating aurora event occurring on 11 February 2008, using the Time History of Events and Macroscale Interactions during Substorms (THEMIS) All-Sky Imager (ASI) array, indicate a spatially and temporally continuous event with a duration of greater than 15h and covering a region with a maximum size of greater than 10h magnetic local time. The optical pulsations are at times locally interrupted or drowned out by auroral substorm activity but are observed in the same location once the discrete aurora recedes. The pulsations following the auroral breakup appear to be brighter and have a larger patch size than before breakup. This suggests that, while the onset of pulsating aurora is not necessarily dependent upon a substorm precursor, the pulsations are affected and possibly enhanced by the substorm process. The long duration of this pulsating aurora event, lasting approximately 8h without interruption as imaged from Gillam station, is significantly longer than the typical 2-3h substorm recovery phase, suggesting that pulsating aurora is not strictly a recovery phase phenomenon. This paper is accompanied by a movie of the THEMIS ASI array data, from 0000 to 1715UT, plotted in mosaic and superimposed onto a map of North America. C1 [Jones, S. L.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Lessard, M. R.; Rychert, K.; Jaynes, A. N.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Spanswick, E.] Los Alamos Natl Lab, Los Alamos, NM USA. [Donovan, E.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. RP Jones, SL (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM sarah.l.jones@nasa.gov RI Jones, Sarah/D-5293-2012; OI Jones, Sarah/0000-0002-3816-4954; Donovan, Eric/0000-0002-8557-4155 FU NASA [NNX08AT38H] FX Research at the University of New Hampshire was supported by NASA grant NNX08AT38H. Ground magnetometer data was provided by the Danish Meteorological Institute (Narsarsuaq) and by the Geological Survey of Canada (Iqaluit) through World Data Center for Geomagnetism, Kyoto. AU and AL indices were provided by the World Data Center for Geomagnetism, Kyoto. NR 38 TC 10 Z9 10 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 2998 EP 3006 DI 10.1002/jgra.50301 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100025 ER PT J AU Samsonov, AA Sibeck, DG AF Samsonov, A. A. Sibeck, D. G. TI Large-scale flow vortices following a magnetospheric sudden impulse SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE sudden impulse; flow vortices; MHD discontinuities ID TRAVELING CONVECTION VORTICES; SOLAR-WIND; INTERPLANETARY SHOCK; THEMIS OBSERVATIONS; DENSITY PULSE; SIMULATION; COMMENCEMENT; PROPAGATION; WAVES AB Global MHD simulations predict the generation of flow vortices on the magnetospheric flanks near the equatorial plane after the impact of solar wind dynamic pressure pulses on the magnetosphere. These vortices are associated with field-aligned currents, having similar senses to those responsible for the main impulse, i.e., the second impulse of the well-known sudden impulse variations at high geomagnetic latitudes. We investigate the evolution of the vortices and show that they result from the interaction of a fast MHD wave and the inner (near-Earth) boundary of numerical models. Near the inner boundary, the Ampere force decelerates plasma flow resulting in two closely related phenomena: the generation of flow vortices and the launch of a reflected fast wave moving sunward. The vortices propagate antisunward and split into several parts during several minutes. The reflected wave interacts with the magnetopause and bow shock and changes its velocity. The interaction between the reflected wave and bow shock results in two new discontinuities moving earthward through the magnetosheath. The first is either a very weak fast rarefaction wave or a weak fast shock, and the second is either a tangential discontinuity or a compound discontinuity with a decrease of the density and magnetic field and an increase of the temperature. We speculate that the inner boundary in simulations may correspond to either the plasmasphere or ionosphere. C1 [Samsonov, A. A.] St Petersburg State Univ, Fac Phys, Dept Earth Phys, St Petersburg 198504, Russia. [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Samsonov, AA (reprint author), St Petersburg State Univ, Fac Phys, Dept Earth Phys, St Petersburg 198504, Russia. EM andre.samsonov@gmail.com RI Samsonov, Andrey/I-7057-2012 OI Samsonov, Andrey/0000-0001-8243-1151 FU NASA FX This work was partly supported by NASA's Guest Investigator program. Simulation results have been provided by the Community Coordinated Modeling Center (http://ccmc.gsfc.nasa.gov) at Goddard Space Flight Center. In figures, we have shown results of the runs "Andrey Samsonov 120507 1" and "Andrey Samsonov 081408 1." NR 41 TC 8 Z9 8 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 3055 EP 3064 DI 10.1002/jgra.50329 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100030 ER PT J AU Cohen, IJ Lessard, MR Kaeppler, SR Bounds, SR Kletzing, CA Streltsov, AV LaBelle, JW Dombrowski, MP Jones, SL Pfaff, RF Rowland, DE Anderson, BJ Korth, H Gjerloev, JW AF Cohen, I. J. Lessard, M. R. Kaeppler, S. R. Bounds, S. R. Kletzing, C. A. Streltsov, A. V. LaBelle, J. W. Dombrowski, M. P. Jones, S. L. Pfaff, R. F. Rowland, D. E. Anderson, B. J. Korth, H. Gjerloev, J. W. TI Auroral Current and Electrodynamics Structure (ACES) observations of ionospheric feedback in the Alfven resonator and model responses SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetosphere-ionosphere coupling; ionospheric feedback instability; Alfven resonator; ACES; rocket; IFI ID MAGNETOSPHERE; INSTABILITY; WAVES; ARCS AB The ACES-High rocket, part of the Auroral Current and Electrodynamics Structure (ACES) mission launched from Poker Flat Research Range on 29 January 2009, obtained the first in situ measurements indicative of both of the observational characteristics associated with the ionospheric feedback instability as it flew through an auroral arc and its associated return current region. ACES-High observed Alfvenic wave structures localized in areas of roughly 10km near the boundaries of the return current region associated with the discrete auroral arc and increased electron density with a temperature characteristic of a cold ionosphere. This density enhancement is believed to be caused by the excavation of plasma from lower altitudes via the ponderomotive force produced by the ionospheric Alfven resonator, as shown by Streltsov and Lotko (2008). While this density is lower than expected from simulations and other observations by as much as an order of magnitude, the ratio of the enhancement to the background density is in agreement with predictions. The observations made by ACES-High agree with the model results by Streltsov and Lotko (2008) but show the localized wave structures only near the boundaries of the return current region and not throughout it. This can be explained by strong small-scale magnetic field-aligned currents that are generated by the interaction between the large-scale downward current and the ionosphere at these boundaries. Finally, a new model, based on that by Streltsov and Marklund (2006), was run with only one downward current region and produced results very similar to the observations seen by ACES-High. C1 [Cohen, I. J.; Lessard, M. R.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03820 USA. [Kaeppler, S. R.; Bounds, S. R.; Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Streltsov, A. V.] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL USA. [LaBelle, J. W.; Dombrowski, M. P.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Jones, S. L.; Pfaff, R. F.; Rowland, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Anderson, B. J.; Korth, H.; Gjerloev, J. W.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD USA. [Gjerloev, J. W.] Univ Bergen, Dept Phys & Technol, Bergen, Norway. RP Cohen, IJ (reprint author), Univ New Hampshire, Ctr Space Sci, Morse Hall,8 Coll Rd, Durham, NH 03820 USA. EM ian.cohen@unh.edu RI Rowland, Douglas/F-5589-2012; Jones, Sarah/D-5293-2012; Cohen, Ian/K-3038-2015; OI Rowland, Douglas/0000-0003-0948-6257; Jones, Sarah/0000-0002-3816-4954; Cohen, Ian/0000-0002-9163-6009; Kletzing, Craig/0000-0002-4136-3348 FU National Aeronautics and Space Administration [NNX07AK01G, NNX11AK71H, NNX10AL17G, NNX12AI44G, NNX10AL18G, NNX07AJ97G] FX The authors would also like to extend our gratefulness to the staff and engineers at NASA Wallops Flight Facility. The work in this paper was supported by several grants from the National Aeronautics and Space Administration: NNX07AK01G, NNX11AK71H, and NNX10AL17G to the University of New Hampshire; NNX12AI44G and NNX10AL18G to Dartmouth College; and NNX07AJ97G to the University of Iowa. NR 22 TC 4 Z9 4 U1 1 U2 9 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 JUN PY 2013 VL 118 IS 6 BP 3288 EP 3296 DI 10.1002/jgra.50348 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100049 ER PT J AU Zhang, H Sibeck, DG Zong, QG Omidi, N Turner, D Clausen, LBN AF Zhang, H. Sibeck, D. G. Zong, Q. -G. Omidi, N. Turner, D. Clausen, L. B. N. TI Spontaneous hot flow anomalies at quasi-parallel shocks: 1. Observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE hot flow anomaly; quasi-parallel shocks; foreshock ID EARTHS BOW SHOCK; GLOBAL HYBRID SIMULATION; FORESHOCK CAVITIES; DIAMAGNETIC CAVITIES; SOLAR-WIND; MAGNETOPAUSE; INSTRUMENT; UPSTREAM AB We present Time History of Events and Macroscale Interactions during Substorms (THEMIS) observations of a Spontaneous Hot Flow Anomaly (SHFA) upstream from the prenoon bow shock at 0431 UT on 12 August 2007. Although the SHFA exhibited the greatly heated and deflected solar wind plasmas used to identify hot flow anomalies (HFAs), it did not result from the standard mechanism invoked for the formation of HFAs, namely the interaction of an interplanetary magnetic field (IMF) discontinuity with the bow shock. We employ THEMIS A, B, C, and D observations to describe the evolution of the event from a proto-SHFA exhibiting regions of depressed magnetic field strength and density but little evidence for plasma heating or flow deflection, to a well-developed SHFA further downstream. These observations show that SHFA can be generated without the presence of an IMF discontinuity and are therefore a new category of HFAs. C1 [Zhang, H.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zong, Q. -G.] Univ Massachusetts Lowell, Ctr Atmospher Res, Lowell, MA USA. [Zong, Q. -G.] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China. [Omidi, N.] Solana Sci Inc, Solana Beach, CA USA. [Turner, D.] Univ Calif Los Angeles, ESS, IGPP, Los Angeles, CA USA. [Clausen, L. B. N.] TU Braunschweig, Inst Geophys & Extraterr Phys, Braunschweig, Germany. RP Zhang, H (reprint author), Univ Alaska, Inst Geophys, 903 Koyukuk Dr,POB 757320, Fairbanks, AK 99775 USA. EM hzhang@gi.alaska.edu RI Turner, Drew/G-3224-2012 FU NSF [AGS-0963111, AGS-0962815, AGS-1007449]; Deutsches Zentrum f. Luft- und Raumfahrt [50OC1102, 50OC1001] FX This work is supported by NSF grants AGS-0963111, AGS-0962815, and AGS-1007449. L.B.N.C. acknowledges funding from the Deutsches Zentrum f. Luft- und Raumfahrt under grants 50OC1102 and 50OC1001. NR 32 TC 19 Z9 19 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 3357 EP 3363 DI 10.1002/jgra.50376 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100055 ER PT J AU Birn, J Hesse, M AF Birn, J. Hesse, M. TI The substorm current wedge in MHD simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE substorm; current wedge; field-aligned currents ID BURSTY BULK FLOWS; FIELD-ALIGNED CURRENTS; PLASMA SHEET; AURORAL STREAMERS; MAGNETIC RECONNECTION; FLUX TUBES; MAGNETOTAIL; TAIL; DIPOLARIZATION; MAGNETOSPHERE AB Using magnetohydrodynamic (MHD) simulations of magnetotail dynamics, we investigate the build-up and evolution of the substorm current wedge (SCW) and its association with plasma flows from the tail. Three different scenarios are considered: the propagation of magnetic flux ropes of artificially reduced entropy (bubbles), and the formation and propagation of bubbles resulting from magnetic reconnection in the near and far tail. The simulations confirm the important role of the entropy reduction in the earthward penetration of bubbles, as well as in the build-up of field-aligned current signatures attributed to the SCW. Low-entropy flow channels can indeed propagate close to the Earth from the distant tail, as suggested recently. However, this requires substantial entropy reduction, presumably from progression of reconnection into the lobes. The major SCW and pressure build-up occurred when the low-entropy flow channels were braked and the flow diverted azimuthally in the near-Earth region. The flows commonly exhibit multiple narrow channels, separated in space and time, whereas the associated increases in B-z (dipolarization) accumulate over a wider spatial range, spreading both azimuthally and radially. This suggests a picture of the SCW as being composed of multiple smaller wedgelets, rather than one big wedge. C1 [Birn, J.] Space Sci Inst, Boulder, CO 80301 USA. [Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Birn, J.] Los Alamos Natl Lab, Los Alamos, NM USA. RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA. EM jbirn@spacescience.org RI feggans, john/F-5370-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU US Department of Energy at Los Alamos; NASA; NSF GEM [1203711]; International Space Science Institute, Bern, Switzerland FX This work was performed mostly at Los Alamos under the auspices of the US Department of Energy, supported by NASA's MMS/SMART Theory and Modeling and SR&T Programs and NSF GEM grant 1203711. JB also acknowledges the hospitality and support of the International Space Science Institute, Bern, Switzerland, and fruitful discussions with Mike Henderson, Los Alamos, and the members of the ISSI team, Larry Kepko, Olaf Amm, Mark Lester, Bob McPherron, Rumi Nakamura, Tuija Pulkkinen, and Victor Sergeev. NR 55 TC 30 Z9 30 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 3364 EP 3376 DI 10.1002/jgra.50187 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100056 ER PT J AU Valek, PW Goldstein, J McComas, DJ Ilie, R Buzulukova, N Fok, MC Perez, JD AF Valek, P. W. Goldstein, J. McComas, D. J. Ilie, R. Buzulukova, N. Fok, M. -C. Perez, J. D. TI Oxygen-hydrogen differentiated observations from TWINS: The 22 July 2009 storm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetic storms; ENAs; Oxygen; TWINS ID THIN CARBON FOILS; RING CURRENT; GEOMAGNETIC STORM; ION COMPOSITION; SOLAR-ACTIVITY; IMAGE MISSION; ENA EMISSION; MAGNETOSPHERE; ALTITUDES AB The 22 July 2009 magnetic storm is the first significant storm during the emergence of the recent prolonged solar cycle minimum. This moderate storm (minimum Dst approximately -78 nT) has received a good deal of attention in the community. We present here global observations of the H and O populations in the inner magnetosphere using Energetic Neutral Atom (ENA) observations from the TWINS mission. We develop and provide the methodology for separating H and O ENAs, based on mass dependent differences in the pulse height distributions of the microchannel plate (MCP) based detectors. We present the first composition separated H and O ENA images at central energies of 16 and 32keV. We also show that TWINS has sufficient angular resolution to separate the High Altitude Emissions (HAEs) from the Low Altitude Emissions (LAEs). We observe that all ENA emissions in this energy range quickly rise, but the O ENAs have a larger relative increase, and stay at elevated levels much longer, well into the recovery phase. C1 [Valek, P. W.; Goldstein, J.; McComas, D. J.] SW Res Inst, San Antonio, TX 78228 USA. [Valek, P. W.; Goldstein, J.; McComas, D. J.] Univ Texas San Antonio, San Antonio, TX USA. [Ilie, R.] Los Alamos Natl Lab, Los Alamos, NM USA. [Buzulukova, N.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Buzulukova, N.; Fok, M. -C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Buzulukova, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Perez, J. D.] Auburn Univ, Auburn, AL 36849 USA. RP Valek, PW (reprint author), SW Res Inst, 6220 Culebra Rd, San Antonio, TX 78228 USA. EM PValek@swri.edu RI Fok, Mei-Ching/D-1626-2012; OI Valek, Philip/0000-0002-2318-8750 FU TWINS mission, NASA's Explorer program FX This work was supported by the TWINS mission, which is a part of NASA's Explorer program. We thank the World Data Center for Geomagnetism, Kyoto for suppling Real Time Dst and AE indices. We also thank the ACE and Wind plasma and magnetometer teams for L1 data and the OMNI data set for their propagation of these data. NR 49 TC 7 Z9 7 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 JUN PY 2013 VL 118 IS 6 BP 3377 EP 3393 DI 10.1002/jgra.50204 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100057 ER PT J AU Christon, SP Hamilton, DC DiFabio, RD Mitchell, DG Krimigis, SM Jontof-Hutter, DS AF Christon, S. P. Hamilton, D. C. DiFabio, R. D. Mitchell, D. G. Krimigis, S. M. Jontof-Hutter, D. S. TI Saturn suprathermal O-2(+) and mass-28(+) molecular ions: Long-term seasonal and solar variation SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Saturn; ion; molecule; season; dust ID E-RING PARTICLES; INNER MAGNETOSPHERE; ENCELADUS; PLASMA; DYNAMICS; PLUME; WATER; DUST; MODEL; REDISTRIBUTION AB Suprathermal singly charged molecular ions, O-2(+) (at similar to 32 Da/e) and the Mass-28 ion group M-28(+) (ions at similar to 28 Da/e, with possible contributions from C2H5+, HCNH+, N-2(+), and/or CO+), are present throughout Saturn's similar to 4-20 Rs (1 Saturn radius, Rs=60,268 km) near-equatorial magnetosphere from mid-2004 until mid-2012. These similar to 83-167 keV/e heavy ions measured by Cassini's CHarge-Energy-Mass Spectrometer have long-term temporal profiles that differ from each other and differ relative to the dominant water group ions, W+ (O+, OH+, H2O+, and H3O+). O-2(+)/W+, initially similar to 0.05, declined steadily until equinox in mid-2009 by a factor of similar to 6, and M-28(+)/W+, initially similar to 0.007, declined similarly until early-2007 by a factor of similar to 2. The O-2(+)/W+ decline is consistent with Cassini's in situ ring-ionosphere thermal ion measurements, and with proposed and modeled seasonal photolysis of Saturn's rings for thermal O-2 and O-2(+). The water ice-dominated main rings and Enceladus plume depositions thereon are the two most likely O-2(+) sources. Enceladus' dynamic plumes, though, have no known long-term dependence. After declining, O-2(+)/W+ and M-28(+)/W+ levels remained low until late-2011 when O-2(+)/W+ increased, but M-28(+)/W+ did not. The O-2(+)/W+ increase was steady and became statistically significant by mid-2012, indicating a clear increase after a decline, that is, a possibly delayed O-2(+) seasonal recovery. Ring insolation is driven by solar UV flux which itself varies with the sun's 11 year activity cycle. The O-2(+)/W+ and M-28(+)/W+ declines are consistent with seasonal ring insolation. No O-2(+)/W+ response to the late-2008 solar-cycle UV minimum and recovery is evident. However, the O-2(+)/W+ recovery from the postequinox baseline levels in late-2011 coincided with a strong solar UV enhancement. We suggest a scenario/framework in which the O-2(+) observations can be understood. C1 [Christon, S. P.] Focused Anal & Res, Columbia, MD 21044 USA. [Hamilton, D. C.; DiFabio, R. D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [DiFabio, R. D.] Univ Louisiana, Dept Phys, Lafayette, LA USA. [Mitchell, D. G.; Krimigis, S. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Krimigis, S. M.] Acad Athens, Athens, Greece. [Jontof-Hutter, D. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Christon, SP (reprint author), Focused Anal & Res, Columbia, MD 21044 USA. EM spchriston@aol.com OI Christon, Stephen/0000-0003-1770-2458; Hamilton, Douglas/0000-0001-6103-8019 FU NASA [NAS5-97271, NNX08BA50G] FX We used the Cassini magnetopause and bow shock crossings list for SOI through 2007 compiled by H. J. McAndrews, S. J. Kanani, A. Masters, and J. C. Cutler. We thank L. J. Spilker, A. Flandes, H. W. Hsu, J. H. Westlake, H. T. Smith, S. Kempf, and J. Vandegriff for their help and useful discussions. S.P.C. thanks NASA for support through contract NAS5-97271 and grant NNX08BA50G. NR 105 TC 5 Z9 5 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 3446 EP 3462 DI 10.1002/jgra.50383 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100062 ER PT J AU Huang, CS de La Beaujardiere, O Roddy, PA Hunton, DE Ballenthin, JO Hairston, MR Pfaff, RF AF Huang, Chao-Song de La Beaujardiere, O. Roddy, P. A. Hunton, D. E. Ballenthin, J. O. Hairston, M. R. Pfaff, R. F. TI Large-scale quasiperiodic plasma bubbles: C/NOFS observations and causal mechanism SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE equatorial ionosphere; plasma bubbles; atmospheric gravity waves ID EQUATORIAL-SPREAD-F; MESOSPHERIC GRAVITY-WAVES; TO-DAY VARIABILITY; NONLINEAR EVOLUTION; VELOCITY SHEAR; IRREGULARITIES; CAMPAIGN; REGION; LAYER; INSTABILITIES AB Large-scale periodic plasma bubbles are often observed by ionospheric radars and satellites. The seeding effect of atmospheric gravity waves has been widely used to explain the generation of periodic plasma bubbles. However, it has not been well understood where the seeding process occurs and how a series of plasma bubbles is triggered. In this study, we present the observations of equatorial plasma bubbles by the Communication/Navigation Outage Forecasting System (C/NOFS) satellite. We show examples of quasiperiodic plasma bubbles in the post-midnight sector, with nearly equal distance of 800-1000km between adjacent bubbles, in 2008 under deep solar minimum conditions. The bubble chain covered a longitudinal range of similar to 7000km between 00:00 and 04:00 LT. Quasiperiodic plasma bubbles were also measured by C/NOFS in the evening sector in 2011 during the ascending phase of the solar activity, and the longitudinal distance between adjacent bubbles was similar to 500km. We propose a causal mechanism to explain the generation of quasiperiodic plasma bubbles. In this scenario, atmospheric gravity waves are generated near the sunset terminator and initiate the Rayleigh-Taylor instability there. The spatial (longitudinal) periodicity of plasma bubbles is determined by the temporal periodicity of the seeding gravity waves. A period of 15-30min of the seeding gravity waves corresponds to a longitudinal separation of 500-1000km between adjacent bubbles. This mechanism provides a reasonable explanation of the observed quasiperiodic plasma bubbles. C1 [Huang, Chao-Song; de La Beaujardiere, O.; Roddy, P. A.; Hunton, D. E.; Ballenthin, J. O.] Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM 87117 USA. [Hairston, M. R.] Univ Texas Dallas, Hanson Ctr Space Sci, Dallas, TX 75230 USA. [Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huang, CS (reprint author), Air Force Res Lab, Space Vehicles Directorate, Bldg 570,Rm 2125,3550 Aberdeen Ave SE, Kirtland AFB, NM 87117 USA. EM chaosong.huang@kirtland.af.mil OI Hairston, Marc/0000-0003-4524-4837 FU AFOSR Task [11RV04COR]; NASA [NNH09AM20I]; Air Force Research Laboratory; Department of Defense Space Test Program; National Aeronautics and Space Administration (NASA); Naval Research Laboratory; Aerospace Corporation FX Work by CSH was supported by the AFOSR Task 11RV04COR and the NASA grant NNH09AM20I. The C/NOFS mission is supported by the Air Force Research Laboratory, the Department of Defense Space Test Program, the National Aeronautics and Space Administration (NASA), the Naval Research Laboratory, and The Aerospace Corporation. NR 43 TC 15 Z9 16 U1 0 U2 5 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 JUN PY 2013 VL 118 IS 6 BP 3602 EP 3612 DI 10.1002/jgra.50338 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100079 ER PT J AU Burkholder, BS Hutchins, ML McCarthy, MP Pfaff, RF Holzworth, RH AF Burkholder, Brian S. Hutchins, Michael L. McCarthy, Michael P. Pfaff, Robert F. Holzworth, Robert H. TI Attenuation of lightning-produced sferics in the Earth-ionosphere waveguide and low-latitude ionosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE lightning; vlf; sferic; wwlln ID COLLISION FREQUENCY; LOCATION NETWORK; C/NOFS SATELLITE; MAGNETIC-FIELD; VLF; PROPAGATION; WHISTLERS; PRECIPITATION; VALIDATION; ALTITUDES AB We compare radio atmospherics (sferics) detected by the World Wide Lightning Location Network (WWLLN) to very low frequency (VLF) whistler waves observed in the low-latitude ionosphere by the Vector Electric Field Instrument of the Communications/Navigation Outage Forecasting System (C/NOFS) satellite. We also model the propagation of these sferics through the Earth-ionosphere waveguide to the subsatellite point using the Long-Wavelength Propagation Capability software and compare this result to the same C/NOFS data set. This unprecedentedly expansive data set allows comparison to theory and prior observation of VLF radio wave propagation in the Earth-ionosphere waveguide and low-latitude ionosphere. We show that WWLLN and C/NOFS observe the well-known effect of variable attenuation with direction within the Earth-ionosphere waveguide. Propagation within the ionosphere is also examined, and a lack of attenuation above 400km is observed. Finally, in comparison to recent works using Detection of Electro-Magnetic Emissions Transmitted from Earthquake Regions (DEMETER) data by Fiser et al. and Chum et al., we find that C/NOFS successfully detects whistlers with comparable amplitudes at much greater distances, compared to those reported for DEMETER. C1 [Burkholder, Brian S.; Hutchins, Michael L.; McCarthy, Michael P.; Holzworth, Robert H.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98107 USA. [Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Burkholder, BS (reprint author), Univ Washington, Dept Earth & Space Sci, 4000 15th Ave NE, Seattle, WA 98107 USA. EM bburk2@uw.edu FU AFOSR [FA955009-1-0309]; NASA [NNX08AD12G]; DARPA [HR0011-10-1-0060] FX The authors wish to thank the World Wide Lightning Location Network (http://wwlln.net), a collaboration among over 50 universities and institutions, for providing the lightning location data used in this paper. This research was supported in part by AFOSR grant FA955009-1-0309, NASA grant NNX08AD12G, and DARPA grant HR0011-10-1-0060. NR 31 TC 4 Z9 4 U1 2 U2 11 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 JUN PY 2013 VL 118 IS 6 BP 3692 EP 3699 DI 10.1002/jgra.50351 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100087 ER PT J AU Christensen, AB Bishop, RL Budzien, SA Hecht, JH Mlynczak, MG Russell, JM Stephan, AW Walterscheid, RW AF Christensen, A. B. Bishop, R. L. Budzien, S. A. Hecht, J. H. Mlynczak, M. G. Russell, J. M., III Stephan, A. W. Walterscheid, R. W. TI Altitude profiles of lower thermospheric temperature from RAIDS/NIRS and TIMED/SABER remote sensing experiments SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Thermosphere; Temperature ID KINETIC TEMPERATURE; SABER EXPERIMENT; BAND SYSTEM; ATMOSPHERE; EMISSIONS; DAYGLOW; MIDDLE; SPHERE AB Thermospheric temperatures derived from limb observations of the O-2 A-Band (0,0) emission spectrum obtained from January-July 2010, with the Remote Atmospheric and Ionospheric Detection System (RAIDS) Near Infrared Spectrometer (NIRS) aboard the International Space Station, are compared to temperature results from the Thermosphere Ionosphere Mesosphere Energetics and Dynamics/Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) experiment. To account for a lack of simultaneous common volume observations, the observed temperatures were scaled by the NRLMSIS-00 model temperatures for comparison. It was found that on average SABER, temperatures are warmer than NIRS at all altitudes between 90 and 140km. In the altitude range 90-100km, the SABER temperatures were warmer than NIRS by similar to 10K consistent with previous validation experiments and in agreement with Optical Spectrograph and Infrared Imaging System (OSIRIS) O-2 A-band comparisons in the polar mesopause region. At higher altitudes, the differences between SABER and NIRS exceed 30K on average. Thus, the NIRS observations reinforce the idea that the SABER temperatures are too warm below similar to 110km; and above that altitude, they are increasingly in error consistent with expectations based on estimated inaccuracies in the retrieval algorithm. Large standard deviations of the SABER and NIRS ratios are reflective of substantial variability of the thermospheric temperatures throughout the region. C1 [Christensen, A. B.] Dixie State Univ, St George, UT 84770 USA. [Bishop, R. L.; Hecht, J. H.; Walterscheid, R. W.] Aerosp Corp, Los Angeles, CA 90009 USA. [Budzien, S. A.; Stephan, A. W.] Naval Res Lab, Washington, DC USA. [Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Russell, J. M., III] Hampton Univ, Sch Sci, Hampton, VA 23668 USA. RP Christensen, AB (reprint author), Dixie State Univ, 225 South 700 East, St George, UT 84770 USA. EM andrew.christensen@aero.org FU Office of Naval Research; Aerospace Corporation Independent Research and Development Program; Aerospace Corporation's Sustained Experimentation and Research for Program Applications; NRL [76-9880]; NASA [NNX11AD71G] FX RAIDS is part of the HICO-RAIDS Experiment Payload (HREP), integrated and flown under the direction of the DOD Space Test Program. RAIDS is a joint project of the Naval Research Laboratory and the Aerospace Corporation, with support from the Office of Naval Research and the Aerospace Corporation Independent Research and Development Program and the Aerospace Corporation's Sustained Experimentation and Research for Program Applications. Scott A. Budzien and Andrew W. Stephan were supported by NRL Base Program work unit 76-9880. We would like to acknowledge the programming support from Dixie College Students Nefi Oliva, Stuart Landsee, Landon Terry, Chris Palmer, and Tucker Fife. This work was supported by NASA grant NNX11AD71G to the Aerospace Corporation and subcontracted to Dixie State College. Thanks also go to Chris Mertens from NASA Langley and the SABER data processing team at GATS, Inc. for providing SABER data. NR 32 TC 7 Z9 7 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 3740 EP 3746 DI 10.1002/jgra.50317 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100092 ER PT J AU Shume, EB Mannucci, AJ Butala, MD Pi, X Valladares, CE AF Shume, E. B. Mannucci, A. J. Butala, M. D. Pi, X. Valladares, C. E. TI Flux tube analysis of L-band ionospheric scintillation SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE equatorial and low latitude ionosphere; ionospheric irregularities; scintillation; spectral analysis ID EQUATORIAL SPREAD-F; PLASMA DEPLETIONS; PHASE SCREEN; SATELLITE; FIELD; IRREGULARITIES; AERONOMY; CAMPAIGN; SPECTRA; IMAGES AB This manuscript presents magnetic flux tube analysis of L-band signal scintillation in the nighttime equatorial and low-latitude ionosphere. Residues of the scintillation index S4 estimated from the L-band signals received from Geostationary Earth Orbit (GEO) satellites are employed in the analysis. The S4 estimates have been shown to be associated with simultaneous GPS VTEC variations derived from JPL's GIPSY-GIM package. We have applied the wavelet decomposition technique simultaneously on the S4 time series in a flux tube over the equatorial and low-latitude regions. The technique decomposes the S4 signal to identify the dominant mode of variabilities and the temporal variations of scintillation-producing irregularities in the context of a flux tube. Statistically significant regions of the wavelet power spectra considered in our study have mainly shown that (a) dominant plasma irregularities associated with S4 variabilities in a flux tube have periods of about 4 to 15 minutes (horizontal irregularity scales of about 24 to 90km). These periods match short period gravity waves, (b) scintillation-producing irregularities are anisotropic along the flux tube and in the east-west direction, and (c) the occurrences of scintillation-producing irregularities along the flux tube indicate that the entire flux tube became unstable. However, plasma instability occurrences were not simultaneous in most cases along the flux tube, there were time delays of various orders. Understanding the attributes of L-band scintillation-producing irregularities could be important for developing measures to mitigate L-band signal degradation. C1 [Shume, E. B.; Mannucci, A. J.; Butala, M. D.; Pi, X.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Valladares, C. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02167 USA. RP Shume, EB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA. EM Esayas.B.Shume@jpl.nasa.gov RI Shume, Esayas/I-3354-2013; OI Shume, Esayas/0000-0002-4696-1283 FU National Aeronautics and Space Administration; NASA; Air Force Research Laboratory [FA8718-09-C-0041]; NSF [ATM-1135675] FX The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. E. B. Shume acknowledges the NPP program administered by the Oak Ridge Associated Universities (ORAU) through a contract with NASA. E. B. Shume thanks B. Iijima for the useful discussion regarding the GEO satellite orbits. One of the authors C. E. Valladares was partially supported by Air Force Research Laboratory contract FA8718-09-C-0041 and NSF grant ATM-1135675. Low-latitude Ionospheric Sensor Network (LISN) is a project led by Boston College in collaboration with the Geophysical Institute of Per and other institutions that provide information in benefit of the scientific community. NR 53 TC 3 Z9 3 U1 3 U2 17 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 JUN PY 2013 VL 118 IS 6 BP 3791 EP 3804 DI 10.1002/jgra.50285 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100096 ER PT J AU Briggs, MS Xiong, SL Connaughton, V Tierney, D Fitzpatrick, G Foley, S Grove, JE Chekhtman, A Gibby, M Fishman, GJ McBreen, S Chaplin, VL Guiriec, S Layden, E Bhat, PN Hughes, M Greiner, J von Kienlin, A Kippen, RM Meegan, CA Paciesas, WS Preece, RD Wilson-Hodge, C Holzworth, RH Hutchins, ML AF Briggs, Michael S. Xiong, Shaolin Connaughton, Valerie Tierney, Dave Fitzpatrick, Gerard Foley, Suzanne Grove, J. Eric Chekhtman, Alexandre Gibby, Melissa Fishman, Gerald J. McBreen, Shelia Chaplin, Vandiver L. Guiriec, Sylvain Layden, Emily Bhat, P. N. Hughes, Maximilian Greiner, Jochen von Kienlin, Andreas Kippen, R. Marc Meegan, Charles A. Paciesas, William S. Preece, Robert D. Wilson-Hodge, Colleen Holzworth, Robert H. Hutchins, Michael L. TI Terrestrial gamma-ray flashes in the Fermi era: Improved observations and analysis methods SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE TGFs; terrestrial gamma-ray flashes; lightning; gamma-ray; Fermi GBM; WWLLN ID OPTICAL TRANSIENT DETECTOR; LIGHTNING LOCATION; BURST; SPACE; AIR AB A new data mode and new analysis methods are used to detect Terrestrial Gamma-ray Flashes (TGFs) with the Fermi Gamma-ray Burst Monitor (GBM) 10 times more frequently than previously. In 1037h of observations at times and over regions for which TGFs are expected, 384 new TGFs were found in addition to the 39 TGFs and two Terrestrial Electron Beam events already detected without the new data mode and methodology. Cosmic ray showers were found to be an important background; they show characteristic signatures in the data of both GBM and the Fermi Large Area Telescope Calorimeter that enable their removal, leaving a sample estimated to consist of approximate to 98% TGFs. The sample includes shorter TGFs than previously found with GBM. The true duration distribution likely contains additional short TGFs because their detection by GBM is limited by detector dead time. One-third of this sample has matches with locations from the World Wide Lightning Location Network (WWLLN)maps of these locations show the geographic and meteorological features more clearly than maps of spacecraft locations. The intrinsic TGF rate is evaluated using the lightning rate maps of the Lightning Imaging Sensor, accounting for the detection efficiency of GBM as a function of spacecraft-source offset, from which we estimate a global TGF rate of approximate to 400,000 per year. With continuous production of data in the new mode we estimate that GBM will detect approximate to 850 TGFs per year. C1 [Briggs, Michael S.; Xiong, Shaolin; Connaughton, Valerie; Chaplin, Vandiver L.; Guiriec, Sylvain; Layden, Emily; Bhat, P. N.; Preece, Robert D.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Briggs, Michael S.; Connaughton, Valerie] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Tierney, Dave; Fitzpatrick, Gerard; Foley, Suzanne; McBreen, Shelia] Univ Coll Dublin, Sch Phys, Dublin 2, Ireland. [Grove, J. Eric] US Naval Res Lab, Space Sci Div, Washington, DC 20375 USA. [Chekhtman, Alexandre] George Mason Univ, Sch Phys, Fairfax, VA 22030 USA. [Gibby, Melissa] Jacobs Engn Grp Inc, Huntsville, VA USA. [Fishman, Gerald J.; Wilson-Hodge, Colleen] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Greiner, Jochen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hughes, Maximilian] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Greiner, Jochen; von Kienlin, Andreas] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kippen, R. Marc] Los Alamos Natl Lab, ISR 1, Los Alamos, NM USA. [Meegan, Charles A.; Paciesas, William S.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Holzworth, Robert H.; Hutchins, Michael L.] Univ Washington, Seattle, WA 98195 USA. RP Briggs, MS (reprint author), CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM michael.briggs@uah.edu OI Preece, Robert/0000-0003-1626-7335 FU Fermi Guest Investigator Program; Irish Research Council for Science, Engineering and Technology; Marie Curie Actions under FP7; Science Foundation Ireland [09-RFP-AST-2400] FX We thank Richard Blakeslee, Garry Case, Martino Marisaldi, David Smith, Steven Cummer and Michael Splitt for discussions or assistance. The Fermi GBM Collaboration acknowledges support for GBM development, operations, and data analysis from National Aeronautics and Space Administration (NASA) in the United States and from the Bundesministerium fur Wirtschaft und Technologie (BMWi)/Deutsches Zentrum fur Luft und Raumfahrt (DLR) in Germany. This work was supported in part by the Fermi Guest Investigator Program. The authors wish to thank the World Wide Lightning Location Network (http://wwlln.net), a collaboration among over 50 universities and institutions, for providing the lightning location data used in this paper. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include NASA and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. G. F. acknowledges the support of the Irish Research Council for Science, Engineering and Technology. S. F. acknowledges the support of the Irish Research Council for Science, Engineering and Technology, co-funded by Marie Curie Actions under FP7. D. T. acknowledges support from Science Foundation Ireland under grant number 09-RFP-AST-2400. The authors thank Nikolai Ostgaard and an anonymous reviewer for their comments, which improved the paper. NR 67 TC 36 Z9 36 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 3805 EP 3830 DI 10.1002/jgra.50205 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100097 ER PT J AU Fejer, BG Tracy, BD Pfaff, RF AF Fejer, Bela G. Tracy, Brian D. Pfaff, Robert F. TI Equatorial zonal plasma drifts measured by the C/NOFS satellite during the 2008-2011 solar minimum SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE electric fields; equatorial ionosphere; equatorial zonal drifts; ionospheric dynamics ID VERTICAL ION DRIFTS; LATENT-HEAT RELEASE; LATITUDE IONOSPHERE; MIDDLE; MODEL; DE-2; ELECTRODYNAMICS; CLIMATOLOGY; JICAMARCA; TIDES AB We use the measurements by the Vector Electric Field Investigation (VEFI) on board the Communication/Navigation Outage Forecasting System (C/NOFS) satellite to study the local time and seasonal- and longitudinal-dependent climatology of equatorial F region zonal plasma drifts during 2008-2011. These drifts are essentially westward during the day and eastward at night. Over Jicamarca Radio Observatory, the satellite measurements are in good agreement with incoherent scatter radar drifts. Our data show strong longitudinal variations, particularly in the South American sector during the solstices. The equinoctial data exhibit short-lived and largely enhanced westward drifts near sunrise and wave-4 structures from the early afternoon to late night equinoctial periods. The nighttime eastward drifts are largest near the western American sector at all seasons. The June solstice postmidnight eastward drifts decrease sharply at longitudes of about 310 degrees and have much smaller values in the entire Eastern Hemisphere. We also briefly discuss the relationship between the longitude-dependent vertical and zonal plasma drifts. C1 [Fejer, Bela G.; Tracy, Brian D.] Utah State Univ, Ctr Atmospher & Space Sci, Logan, UT 84322 USA. [Pfaff, Robert F.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Fejer, BG (reprint author), Utah State Univ, Ctr Atmospher & Space Sci, 4405 Old Main Hill, Logan, UT 84322 USA. EM bela.fejer@usu.edu FU Aeronomy Program, Division of Atmospheric Sciences of the National Science Foundation [AGS-1068104]; NASA [NNH12C02C, NNX09ANSSG]; NSF through Cornell University [AGS-0905448] FX This work was supported by the Aeronomy Program, Division of Atmospheric Sciences of the National Science Foundation through grant AGS-1068104 and by NASA through grants NNH12C02C and NNX09ANSSG. The Jicamarca Radio Observatory is a facility of the Instituto Geofisico del Peru and is operated with support from the NSF cooperative agreement AGS-0905448 through Cornell University. NR 40 TC 8 Z9 8 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2013 VL 118 IS 6 BP 3891 EP 3897 DI 10.1002/jgra.50382 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UQ UT WOS:000325217100104 ER PT J AU Guhathakurta, M Davila, JM Gopalswamy, N AF Guhathakurta, Madhulika Davila, Joseph M. Gopalswamy, Nat TI The International Space Weather Initiative (ISWI) SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE space weather C1 [Guhathakurta, Madhulika] NASA, Living With A Star Program, Washington, DC 20546 USA. [Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Guhathakurta, M (reprint author), NASA, Living With A Star Program, Washington, DC 20546 USA. EM madhulika.guhathakurta@nasa.gov NR 3 TC 1 Z9 1 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN PY 2013 VL 11 IS 6 BP 327 EP 329 DI 10.1002/swe.20048 PG 3 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 231OI UT WOS:000325426100001 ER PT J AU Evans, RM Pulkkinen, AA Zheng, YH Mays, ML Taktakishvili, A Kuznetsova, MM Hesse, M AF Evans, Rebekah M. Pulkkinen, Antti A. Zheng, Yihua Mays, M. Leila Taktakishvili, Aleksandre Kuznetsova, Maria M. Hesse, Michael TI The SCORE Scale: A Coronal Mass Ejection Typification System Based On Speed SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Editorial Material DE coronal mass ejection C1 [Evans, Rebekah M.; Pulkkinen, Antti A.; Zheng, Yihua; Mays, M. Leila; Taktakishvili, Aleksandre; Kuznetsova, Maria M.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pulkkinen, Antti A.] NASA, Space Weather Res Ctr, Goddard Space Flight Ctr, Greenbelt, MD USA. [Mays, M. Leila; Taktakishvili, Aleksandre] Catholic Univ Amer, Washington, DC 20064 USA. [Kuznetsova, Maria M.] NASA, Community Coordinated Modeling Ctr, Goddard Space Flight Ctr, Greenbelt, MD USA. [Hesse, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Evans, RM (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM rebekah.e.frolov@nasa.gov RI feggans, john/F-5370-2012 NR 0 TC 7 Z9 7 U1 2 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN PY 2013 VL 11 IS 6 BP 333 EP 334 DI 10.1002/swe.20058 PG 2 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 231OI UT WOS:000325426100003 ER PT J AU Joyce, CJ Schwadron, NA Wilson, JK Spence, HE Kasper, JC Golightly, M Blake, JB Mazur, J Townsend, LW Case, AW Semones, E Smith, S Zeitlin, CJ AF Joyce, C. J. Schwadron, N. A. Wilson, J. K. Spence, H. E. Kasper, J. C. Golightly, M. Blake, J. B. Mazur, J. Townsend, L. W. Case, A. W. Semones, E. Smith, S. Zeitlin, C. J. TI Validation of PREDICCS using LRO/CRaTER observations during three major solar events in 2012 SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE radiation model; doserate; modulation potential AB PREDICCS (Predictions of Radiation from Release, EMMREM, and Data Incorporating the CRaTER, COSTEP and other SEP measurements, prediccs.sr.unh.edu) is an online system designed to provide a near real-time characterization of the radiation environment of the inner heliosphere. PREDICCS utilizes data from various satellites in conjunction with numerical models such as the Earth-Moon-Mars Radiation Environment Module (EMMREM) to produce dose rate and particle flux data at the Earth, Moon and Mars. The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument launched aboard the Lunar Reconnaissance Orbiter (LRO) spacecraft in 2009 and designed to measure energetic particle radiation, offers an opportunity to test the capability of PREDICCS to accurately describe the lunar radiation environment. We provide comparisons between dose rates produced by PREDICCS with those measured by CRaTER during three major solar energetic particle (SEP) events that occurred in 2012. In addition, using EMMREM data products together with our archive of measured CRaTER dose rates, we compute the modulation potential at the Moon throughout the LRO mission and, using this, compute the background GCR dose rate during each event. We demonstrate reasonable agreement between PREDICCS and CRaTER dose rates and come to the conclusion that PREDICCS provides credible characterization of the lunar radiation environment. This study represents the first multi-event validation, via in situ measurement, of radiation models such as EMMREM, which should prove to be valuable in future efforts in risk assessment and in the study of radiation in the inner heliosphere. C1 [Joyce, C. J.; Schwadron, N. A.; Wilson, J. K.; Spence, H. E.; Golightly, M.; Smith, S.] Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA. [Kasper, J. C.; Case, A. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blake, J. B.] Aerosp Corp, Los Angeles, CA 90009 USA. [Mazur, J.] Aerosp Corp, Space Sci Dept Chantilly, Chantilly, VA USA. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Semones, E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zeitlin, C. J.] SW Res Inst, Boulder, CO USA. RP Joyce, CJ (reprint author), Univ New Hampshire, Dept Phys, Ctr Space Sci, 39 Coll Rd, Durham, NH 03824 USA. EM cjl46@unh.edu OI Spence, Harlan/0000-0002-2526-2205 FU NASA LRO/CRaTER/PREDICCS Project [NNG11PA03C]; NSF/FESD Sun-to-Ice Project [AGS1135432]; NASA/LWS/NSF EMMREM Project [NNX11AC06G] FX This work is supported by NASA LRO/CRaTER/PREDICCS Project (Contract NNG11PA03C), the NSF/FESD Sun-to-Ice Project (Grant AGS1135432), and the NASA/LWS/NSF EMMREM Project (Grant NNX11AC06G). We thank the ACE SIS instrument team and the ACE Science Center for providing the ACE data used here. NR 10 TC 9 Z9 9 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN PY 2013 VL 11 IS 6 BP 350 EP 360 DI 10.1002/swe.20059 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 231OI UT WOS:000325426100007 ER PT J AU Pulkkinen, A Rastatter, L Kuznetsova, M Singer, H Balch, C Weimer, D Toth, G Ridley, A Gombosi, T Wiltberger, M Raeder, J Weigel, R AF Pulkkinen, A. Rastaetter, L. Kuznetsova, M. Singer, H. Balch, C. Weimer, D. Toth, G. Ridley, A. Gombosi, T. Wiltberger, M. Raeder, J. Weigel, R. TI Community-wide validation of geospace model ground magnetic field perturbation predictions to support model transition to operations SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE model transition; geomagnetically induced currents; model validation ID IONOSPHERE-THERMOSPHERE MODEL; HORIZONTAL GEOMAGNETIC-FIELD; EXPLORER 12 OBSERVATIONS; SOLAR-WIND; CIRCULATION MODEL; SPACE WEATHER; MAGNETOSPHERIC MODEL; GLOBAL SIMULATION; ELECTRIC-FIELDS; MHD SIMULATION AB In this paper we continue the community-wide rigorous modern space weather model validation efforts carried out within GEM, CEDAR and SHINE programs. In this particular effort, in coordination among the Community Coordinated Modeling Center (CCMC), NOAA Space Weather Prediction Center (SWPC), modelers, and science community, we focus on studying the models' capability to reproduce observed ground magnetic field fluctuations, which are closely related to geomagnetically induced current phenomenon. One of the primary motivations of the work is to support NOAA SWPC in their selection of the next numerical model that will be transitioned into operations. Six geomagnetic events and 12 geomagnetic observatories were selected for validation. While modeled and observed magnetic field time series are available for all 12 stations, the primary metrics analysis is based on six stations that were selected to represent the high-latitude and mid-latitude locations. Events-based analysis and the corresponding contingency tables were built for each event and each station. The elements in the contingency table were then used to calculate Probability of Detection (POD), Probability of False Detection (POFD) and Heidke Skill Score (HSS) for rigorous quantification of the models' performance. In this paper the summary results of the metrics analyses are reported in terms of POD, POFD and HSS. More detailed analyses can be carried out using the event by event contingency tables provided as an online appendix. An online interface built at CCMC and described in the supporting information is also available for more detailed time series analyses. C1 [Pulkkinen, A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Pulkkinen, A.; Rastaetter, L.; Kuznetsova, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Singer, H.; Balch, C.] NOAA, Space Weather Predict Ctr, Boulder, CO USA. [Weimer, D.] Virginia Polytech Inst & State Univ, Ctr Space Sci & Engn Res, Blacksburg, VA 24061 USA. [Toth, G.; Ridley, A.; Gombosi, T.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Raeder, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Raeder, J.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Weigel, R.] George Mason Univ, Dept Computat & Data Sci, Fairfax, VA 22030 USA. RP Pulkkinen, A (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA. EM antti.a.pulkkinen@nasa.gov RI Toth, Gabor/B-7977-2013; Wiltberger, Michael/B-8781-2008; Rastaetter, Lutz/D-4715-2012; Ridley, Aaron/F-3943-2011; Gombosi, Tamas/G-4238-2011 OI Toth, Gabor/0000-0002-5654-9823; Wiltberger, Michael/0000-0002-4844-3148; Rastaetter, Lutz/0000-0002-7343-4147; Ridley, Aaron/0000-0001-6933-8534; Gombosi, Tamas/0000-0001-9360-4951 NR 95 TC 23 Z9 23 U1 3 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN PY 2013 VL 11 IS 6 BP 369 EP 385 DI 10.1002/swe.20056 PG 17 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 231OI UT WOS:000325426100009 ER PT J AU Patel, A Brown, AD Hsieh, WT Stevenson, T Moseley, SH U-yen, K Ehsan, N Barrentine, E Manos, G Wollack, EJ AF Patel, Amil Brown, Ari-David Hsieh, Wen-Ting Stevenson, Thomas Moseley, S. Harvey U-yen, Kongpop Ehsan, Negar Barrentine, Emily Manos, George Wollack, Edward J. TI Fabrication of MKIDS for the MicroSpec Spectrometer SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Microstrip devices; microwave kinetic inductance detector (MKID); molybdenum nitride; niobium; spectrometer; wafer bonding ID ARRAYS AB Microspec is a new class of submillimeter and millimeter (250-700 mu m wavelength) spectrometer, in which the wavelength separation and detection of incident light is done on a single substrate. The instrument is designed for space exploration by offering high spectral resolving power over a broad band, while being orders of magnitude smaller in mass and volume than the present state-of-the-art. The key enabling components for Microspec are background-limited microwave kinetic inductance detectors, which operate over the full bandwidth of the spectrometer. Here we present our fabrication strategy for making these sensitive detectors. A microstrip architecture utilizing a 0.45-mu m crystalline silicon dielectric with a molybdenum nitride kinetic inductor material has been adopted. We have optimized wafer-scale lithographic patterning, and have developed processes that allow us to minimize surface roughness that may contribute to detector noise. Additionally, we have optimized the low-temperature wafer bonding process; this process allows us to build superconductors on both sides of the silicon dielectric layer. We present a final fabricated device and resonator operation at cryogenic temperatures. C1 [Patel, Amil; Brown, Ari-David; Hsieh, Wen-Ting; Stevenson, Thomas; Moseley, S. Harvey; U-yen, Kongpop; Ehsan, Negar; Barrentine, Emily; Manos, George; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Patel, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM amil.a.patel@nasa.gov; ari.d.brown@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA ROSES-APRA program; GSFC IRAD program FX This work was carried out at NASA Goddard Space Flight Center and was supported in part by the NASA ROSES-APRA program and the GSFC IRAD program. NR 11 TC 4 Z9 4 U1 2 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2400404 DI 10.1109/TASC.2013.2240152 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100069 ER PT J AU House, CH Oehler, DZ Sugitani, K Mimura, K AF House, C. H. Oehler, D. Z. Sugitani, K. Mimura, K. TI Carbon isotopic analyses of ca. 3.0 Ga microstructures imply planktonic autotrophs inhabited Earth's early oceans SO GEOLOGY LA English DT Article ID INDIVIDUAL PRECAMBRIAN MICROFOSSILS; BARBERTON GREENSTONE-BELT; STRELLEY POOL FORMATION; WESTERN-AUSTRALIA; PILBARA CRATON; SOUTH-AFRICA; BIOGENICITY; SIGNATURES; EVOLUTION; FRACTIONATION AB The ca. 3 Ga Farrel Quartzite (FQ, Western Australia) contains possible organic microfossils of unusual spindle-like morphology that are surprisingly large and complex, preserved along with spheroids. The unusual nature of the possible fossils, coupled with their antiquity, makes their interpretation as biogenic difficult and debatable. Here, we report 32 in situ carbon isotopic analyses of 15 individual FQ specimens. The spheroids and the spindle-like forms have a weighted mean delta C-13 value of -37 parts per thousand, an isotopic composition that is quite consistent with a biogenic origin. Both the spheroids and the spindle-like structures are isotopically distinct from the background organic matter in the same thin section (weighted mean delta C-13 value of -33 parts per thousand), which shows that the preserved microstructures are not pseudofossils formed from physical reprocessing of the bulk sedimentary organic material. When considered along with published morphological and chemical studies, these results indicate that the FQ microstructures are bona fide microfossils, and support the interpretation that the spindles were planktonic. Our results also provide metabolic constraints that imply most of these preserved microorganisms were autotrophic. The existence of similar spindles in the ca. 3.4 Ga Strelley Pool Formation of Australia and the ca. 3.4 Ga Onverwacht Group of South Africa suggests that the spindle-containing microbiota may be one of the oldest, morphologically preserved examples of life. If this is the case, then the FQ structures represent the remains of a cosmopolitan biological experiment that appears to have lasted for several hundred million years, starting in the Paleoarchean. C1 [House, C. H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [House, C. H.] Penn State Univ, Astrobiol Res Ctr, University Pk, PA 16802 USA. [Oehler, D. Z.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. [Sugitani, K.] Nagoya Univ, Grad Sch Environm Studies, Dept Environm Engn & Architecture, Nagoya, Aichi 4648601, Japan. [Mimura, K.] Nagoya Univ, Grad Sch Environm Studies, Dept Earth & Environm Sci, Nagoya, Aichi 4648601, Japan. RP House, CH (reprint author), Penn State Univ, Dept Geosci, 220 Deike Bldg, University Pk, PA 16802 USA. EM chrishouse@psu.edu; dorothy.z.oehler@nasa.gov RI UCLA, SIMS/A-1459-2011 FU NASA Astrobiology Institute [NNA09DA76A]; Astromaterials Research and Exploration Science Directorate at Johnson Space Center; Japan Society for the Promotion of Science [22340149, 24654162] FX We thank A. K. Schmitt and K. D. McKeegan for assistance with measurements, J.W. Schopf for information from his Raman studies, and T. Nagaoka for preparation of the thin sections. This work was funded by the NASA Astrobiology Institute (NNA09DA76A), and by support from the Astromaterials Research and Exploration Science Directorate at Johnson Space Center. The UCLA facility is partly supported by the Earth Sciences Instrumentation and Facilities Program, National Science Foundation. Sugitani received support from the Japan Society for the Promotion of Science (Japan-Australia Joint Research Program and Grant-in-Aid numbers 22340149 and 24654162). NR 33 TC 13 Z9 13 U1 0 U2 24 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD JUN PY 2013 VL 41 IS 6 BP 651 EP 654 DI 10.1130/G34055.1 PG 4 WC Geology SC Geology GA 203DF UT WOS:000323269800007 ER PT J AU Warner, NH Sowe, M Gupta, S Dumke, A Goddard, K AF Warner, Nicholas H. Sowe, Mariam Gupta, Sanjeev Dumke, Alexander Goddard, Kate TI Fill and spill of giant lakes in the eastern Valles Marineris region of Mars SO GEOLOGY LA English DT Article ID INTERIOR LAYERED DEPOSITS; ORIGIN; CRATER AB The existence of Hesperian age (3.7-3.4 Ga) surface water bodies on Mars is a contentious issue, often conflicting with favored climate models. Extensive lakes are proposed to have filled parts of Valles Marineris during this period, yet evidence for their presence and temporal continuity is poorly constrained. Here we report geomorphic and chronologic evidence for the initiation and demise of a voluminous lake system within the basins of eastern Valles Marineris. We find that independent, kilometer-deep lakes were present here well after the wetter, global climate optimum that characterized the previous Noachian epoch (4.1-3.7 Ga). Relative and impact crater chronologies of flood channels emerging from lake basins indicate relatively late lake spillover in the Early Amazonian (ca. 3.0 Ga). Drawdown of the lake and cessation of interbasin sedimentation may be recorded by a similar Early Amazonian (ca. 3.1 Ga) crater retention age on the surface of Capri Mensa, a 4-km-tall, sulfate-bearing interior layered deposit. The topography data demonstrate that incision of the bedrock barriers between the basins during spillover was driven by a dramatic local base-level difference between the lake surface and downstream basin floors. We postulate that the lake spillover process created an integrated drainage routing system between a voluminous equatorial water supply and the northern plains basin. C1 [Warner, Nicholas H.; Gupta, Sanjeev; Goddard, Kate] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Sowe, Mariam; Dumke, Alexander] Free Univ Berlin, Inst Geol Sci Planetary Sci & Remote Sensing, D-12249 Berlin, Germany. RP Warner, NH (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Nicholas.H.Warner@jpl.nasa.gov OI Dumke, Alexander/0000-0002-2709-3169 FU UK Science and Technology Facilities Council (STFC) [ST/F003099/1]; Helmholtz Alliance "Planetary Evolution and Life''; Deutsche Forschungsgemeinschaft [SO 1143/1]; German Space Agency [50QM1001]; German Federal Ministry of Economics and Technology; STFC; Jet Propulsion Laboratory-California Institute of Technology; NASA FX We thank the HRSC (High-Resolution Stereo Camera) team at Freie Universitat Berlin, the German Aerospace Centre (DLR), the European Space Agency (ESA), as well as the CTX (Context Camera) and HiRISE (High Resolution Imaging Science Experiment) teams. Warner and Gupta were supported by the UK Science and Technology Facilities Council (STFC) under grant ST/F003099/1. Sowe was funded in part by the Helmholtz Alliance "Planetary Evolution and Life'' and Deutsche Forschungsgemeinschaft travel grant SO 1143/1. Dumke was supported by German Space Agency grant 50QM1001 (HRSC on Mars Express) on behalf of the German Federal Ministry of Economics and Technology. Goddard was funded by an STFC doctoral studentship. Warner was partially supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory-California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. We thank Brian Hynek, Samuel C. Schon, and two anonymous reviewers for their comments. NR 21 TC 19 Z9 19 U1 0 U2 17 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD JUN PY 2013 VL 41 IS 6 BP 675 EP 678 DI 10.1130/G34172.1 PG 4 WC Geology SC Geology GA 203DF UT WOS:000323269800013 ER PT J AU Ekstrand, AL Webley, PW Garay, MJ Dehn, J Prakash, A Nelson, DL Dean, KG Steensen, T AF Ekstrand, Angela L. Webley, Peter W. Garay, Michael J. Dehn, Jonathan Prakash, Anupma Nelson, David L. Dean, Kenneson G. Steensen, Torge TI A multi-sensor plume height analysis of the 2009 Redoubt eruption SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Remote sensing; Redoubt; Ash clouds; MISR; MODIS; AVHRR ID VOLCANIC ASH CLOUDS; SATELLITE-OBSERVATIONS; WEATHER RADAR; RETRIEVAL; DYNAMICS; ALASKA; MODEL; MISR; TOP AB During an explosive volcanic eruption, accurately determining the height of a volcanic plume or cloud is essential to accurately forecast its motion because volcanic ash transport and dispersion models require the initial plume height as an input parameter. The direct use of satellite infrared temperatures for height determination, one of the most commonly employed methods at the Alaska Volcano Observatory, often does not yield unique solutions for height. This result is documented here for the 2009 eruption of Redoubt Volcano. Satellite temperature heights consistently underestimated the height of ash plumes in comparison to other methods such as ground-based radar and Multi-angle Imaging SpectroRadiometer (MISR) stereo heights. For ash plumes below the tropopause, increasing transparency of a plume begins to affect the accuracy of simple temperature height retrievals soon after eruption. With decreasing opacity, plume temperature heights become increasingly inaccurate. Comparison with dispersion models and aircraft gas flight data confirms that radar and MISR stereo heights are more accurate than basic satellite temperature heights. Even in the cases in which satellite temperature results appeared to be relatively accurate (e.g., for plumes below the tropopause), a mixed signal of plume and ground radiation still presented an issue for almost every event studied. This was true regardless of the fact that a band differencing method was used to remove presumably translucent pixels. The data presented here make a strong case for the use of data fusion in volcano monitoring, as there is a need to confirm satellite temperature heights with other height data. If only basic satellite temperature heights are available for a given eruption, then these heights must be considered with a significant margin of error. (c) 2012 Elsevier B.V. All rights reserved. C1 [Ekstrand, Angela L.; Webley, Peter W.; Dehn, Jonathan; Prakash, Anupma; Dean, Kenneson G.; Steensen, Torge] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Ekstrand, Angela L.; Webley, Peter W.; Dehn, Jonathan; Dean, Kenneson G.; Steensen, Torge] Univ Alaska Fairbanks, Alaska Volcano Observ, Fairbanks, AK 99775 USA. [Garay, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nelson, David L.] Raytheon Co, Pasadena, CA 91101 USA. RP Ekstrand, AL (reprint author), Univ Alaska Fairbanks, Inst Geophys, Alaska Volcano Observ, 903 Koyukuk Dr, Fairbanks, AK 99775 USA. EM angela.ekstrand@gi.alaska.edu RI Webley, Peter/F-8238-2015 OI Webley, Peter/0000-0001-5327-8151 FU American Reinvestment and Recovery Act; Alaska Space Grant Program; National Aeronautics and Space Administration FX We would like to thank Lovro Valcic (AVO/UAF-GI) and Scott McFarlane (AVO/UAF-GI) for assistance in obtaining and processing AVHRR and MODIS satellite imagery, David McAlpin (UAF-GI) for processing of the DEM data, Jeremy Harbeck for assistance with programming and computational analysis in IDL, David Schneider (USGS) for providing radar data, Peter Kelly (USGS) for providing gas flight data, and Steve McNutt (AVO/UAF-GI) for providing seismic data. Thanks to Ralph Kahn (NASA GSFC) and Michael Pavolonis (NOAA) and one anonymous reviewer for helpful comments and feedback. This work was supported in part by The American Reinvestment and Recovery Act, as well as the Alaska Space Grant Program. Portions of this work were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 59 TC 5 Z9 5 U1 1 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD JUN 1 PY 2013 VL 259 SI SI BP 170 EP 184 DI 10.1016/j.jvolgeores.2012.09.008 PG 15 WC Geosciences, Multidisciplinary SC Geology GA 195FU UT WOS:000322688500013 ER PT J AU Mersel, MK Smith, LC Andreadis, KM Durand, MT AF Mersel, Matthew K. Smith, Laurence C. Andreadis, Konstantinos M. Durand, Michael T. TI Estimation of river depth from remotely sensed hydraulic relationships SO WATER RESOURCES RESEARCH LA English DT Article DE hydraulic geometry; river depth; surface water and ocean topography; SWO; slope break ID SATELLITE RADAR ALTIMETRY; SYNTHETIC-APERTURE RADAR; WATER-LEVEL CHANGES; AMAZON FLOODPLAIN; WETLAND DYNAMICS; INUNDATION AREA; SURFACE-WATER; GEOMETRY; DISCHARGE; BASIN AB The Surface Water and Ocean Topography (SWOT) radar interferometer satellite mission will provide unprecedented global measurements of water surface elevation (h) for inland water bodies. However, like most remote sensing technologies SWOT will not observe river channel bathymetry below the lowest observed water surface, thus limiting its value for estimating river depth and/or discharge. This study explores if remotely sensed observations of river inundation width and h alone, when accumulated over time, may be used to estimate this unmeasurable flow depth. To test this possibility, synthetic values of h and either cross-sectional flow width (w) or effectivewidth (We, inundation area divided by reach length) are extracted from 1495 previously surveyed channel cross-sections for the Upper Mississippi, Illinois, Rio Grande, and Ganges-Brahmaputra river systems, and from 62 km of continuously acquired sonar data for the Upper Mississippi. Two proposed methods (called "Linear" and "Slope-Break") are tested that seek to identify a small subset of geomorphically "optimal" locations where w or We covary strongly with h, such that they may be usefully extrapolated to estimate mean cross-sectional flow depth (d). While the simplest Linear Method is found to have considerable uncertainty, the Slope-Break Method, identifying locations where two distinct hydraulic relationships are identified (one for moderate to high flows and one for low flows), holds promise. Useful slope breaks were discovered in all four river systems, ranging from 6 (0.04%) to 242 (16%) of the 1495 studied cross-sections, assuming channel bathymetric exposures ranging from 20% to 95% of bankfull conditions, respectively. For all four rivers, the derived depth estimates from the Slope-Break Method have root mean squared errors (RMSEs) of <20% (relative to bankfull mean depth) assuming at least one channel bathymetry exposure of similar to 25% or greater. Based on historic discharge records and HEC-RAS hydraulic modeling, the Upper Mississippi and Rio Grande rivers experience adequate channel exposures at least similar to 60% and similar to 42% of the time, respectively. For the Upper Mississippi, so-called "reach-averaging" (spatial averaging along some predetermined river length) of native-resolution h and We values reduces both RMSE and longitudinal variability in the derived depth estimates, especially at reach-averaging lengths of similar to 1000-2000 m. These findings have positive implications for SWOT and other sensors attempting to estimate river flow depth and/or discharge solely from incomplete, remotely sensed hydraulic variables, and suggest that useful depth retrievals can be obtained within the spatial and temporal constraints of satellite observations. C1 [Mersel, Matthew K.; Smith, Laurence C.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA. [Smith, Laurence C.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Andreadis, Konstantinos M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Durand, Michael T.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Durand, Michael T.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. RP Mersel, MK (reprint author), Cold Reg Res & Engn Lab, RS GIS 103,72 Lyme Rd, Hanover, NH 03755 USA. EM mmersel@ucla.edu RI Durand, Michael/D-2885-2013; Smith, Laurence/E-7785-2012 OI Smith, Laurence/0000-0001-6866-5904 FU NASA Physical Oceanography Program [NNX10AE96G] FX This research was funded by the NASA Physical Oceanography Program (grant NNX10AE96G), managed by Eric Lindstrom. In situ cross-section data for the Ganges-Brahmaputra river system was provided by Faissal Hossain (Tennessee Technical University) as part of a Memorandum of Understanding between the Institute of Water Modeling-Bangladesh and Tennessee Technical University. In situ cross-section data for the Rio Grande (surveyed by Tetra Tech Inc.) and for the Upper Mississippi and Illinois rivers (surveyed by the U. S. Army Corps of Engineers) was provided to the authors by Edward Beighley (FM Global). The continuous in situ bathymetric data set for the Upper Mississippi was provided by the USGS, as part of the Long Term Resource Monitoring Program. The authors thank Doug Alsdorf, Paul Bates, and one anonymous reviewer for their constructive feedback on this paper. NR 51 TC 19 Z9 19 U1 3 U2 49 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 JUN PY 2013 VL 49 IS 6 BP 3165 EP 3179 DI 10.1002/wrcr.20176 PG 15 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 189BF UT WOS:000322241300007 ER PT J AU Corron, NJ Stahl, MT Harrison, RC Blakely, JN AF Corron, Ned J. Stahl, Mark T. Harrison, R. Chase Blakely, Jonathan N. TI Acoustic detection and ranging using solvable chaos SO CHAOS LA English DT Article ID COLPITTS OSCILLATOR; AMBIGUITY FUNCTIONS; RADAR; SIGNALS AB Acoustic experiments demonstrate a novel approach to ranging and detection that exploits the properties of a solvable chaotic oscillator. This nonlinear oscillator includes an ordinary differential equation and a discrete switching condition. The chaotic waveform generated by this hybrid system is used as the transmitted waveform. The oscillator admits an exact analytic solution that can be written as the linear convolution of binary symbols and a single basis function. This linear representation enables coherent reception using a simple analog matched filter and without need for digital sampling or signal processing. An audio frequency implementation of the transmitter and receiver is described. Successful acoustic ranging measurements in the presence of noise and interference from a second chaotic emitter are presented to demonstrate the viability of the approach. C1 [Corron, Ned J.; Harrison, R. Chase; Blakely, Jonathan N.] US Army Aviat & Missile Res Dev & Engn Ctr, Charles M Bowden Lab, Redstone Arsenal, AL 35898 USA. [Stahl, Mark T.] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Corron, NJ (reprint author), US Army Aviat & Missile Res Dev & Engn Ctr, Charles M Bowden Lab, Redstone Arsenal, AL 35898 USA. OI Corron, Ned/0000-0002-3232-5024 NR 21 TC 8 Z9 8 U1 0 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 1054-1500 J9 CHAOS JI Chaos PD JUN PY 2013 VL 23 IS 2 AR 023119 DI 10.1063/1.4808252 PG 7 WC Mathematics, Applied; Physics, Mathematical SC Mathematics; Physics GA 174HR UT WOS:000321146500019 PM 23822484 ER PT J AU MacLachlan, GA Shenoy, A Sonbas, E Dhuga, KS Cobb, BE Ukwatta, TN Morris, DC Eskandarian, A Maximon, LC Parke, WC AF MacLachlan, G. A. Shenoy, A. Sonbas, E. Dhuga, K. S. Cobb, B. E. Ukwatta, T. N. Morris, D. C. Eskandarian, A. Maximon, L. C. Parke, W. C. TI Minimum variability time-scales of long and short GRBs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; methods: data analysis; methods: statistical; gamma-ray burst: general ID GAMMA-RAY BURSTS; FRACTIONAL BROWNIAN MOTIONS; LUMINOSITY RELATION; LIGHT CURVES; DURATION; PULSES; ACCRETION; LAG AB We have investigated the time variations in the light curves from a sample of long and short Fermi/GBM gamma-ray bursts (GRBs) using an impartial wavelet analysis. The results indicate that in the source frame, the variability time-scales for long bursts differ from that for short bursts, variabilities of the order of a few milliseconds are not uncommon and an intriguing relationship exists between the minimum variability time and the burst duration. C1 [MacLachlan, G. A.; Shenoy, A.; Dhuga, K. S.; Cobb, B. E.; Ukwatta, T. N.; Morris, D. C.; Eskandarian, A.; Maximon, L. C.; Parke, W. C.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Sonbas, E.] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey. [Sonbas, E.; Ukwatta, T. N.; Morris, D. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ukwatta, T. N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Morris, D. C.] Univ Virgin Isl, Dept Phys, St Thomas, VI USA. RP MacLachlan, GA (reprint author), George Washington Univ, Dept Phys, Washington, DC 20052 USA. EM maclach@gwu.edu FU NASA [NNX11AE36G] FX The NASA grant NNX11AE36G provided partial support for this work and is gratefully acknowledged. The authors, in particular GAM and KSD, acknowledge very useful discussions with Jon Hakkila and Narayan Bhat early in the manuscript development. GAM and KSD also acknowledge helpful correspondences with Jeffery Scargle. NR 38 TC 14 Z9 14 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 2 BP 857 EP 865 DI 10.1093/mnras/stt241 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300001 ER PT J AU Jerzykiewicz, M Lehmann, H Niemczura, E Molenda-Zakowicz, J Dymitrov, W Fagas, M Guenther, DB Hartmann, M Hrudkova, M Kaminski, K Moffat, AFJ Kuschnig, R Leto, G Matthews, JM Rowe, JF Rucinski, SM Sasselov, D Weiss, WW AF Jerzykiewicz, M. Lehmann, H. Niemczura, E. Molenda-Zakowicz, J. Dymitrov, W. Fagas, M. Guenther, D. B. Hartmann, M. Hrudkova, M. Kaminski, K. Moffat, A. F. J. Kuschnig, R. Leto, G. Matthews, J. M. Rowe, J. F. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI mu Eridani from MOST star and from the ground: an orbit, the SPB component's fundamental parameters and the SPB frequencies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: eclipsing; binaries: spectroscopic; stars: early-type; stars: individual: mu Eridani; stars: oscillations ID B-TYPE STARS; EMPIRICAL EFFECTIVE TEMPERATURES; SOLAR MODEL PROBLEM; BOLOMETRIC CORRECTIONS; RADIAL-VELOCITIES; ECLIPSING BINARIES; BETA PHOTOMETRY; SURFACE GRAVITY; NU-ERIDANI; F-STARS AB MOST time series photometry of mu Eri, an SB1 eclipsing binary with a rapidly rotating SPB primary, is reported and analysed. The analysis yields a number of sinusoidal terms, mainly due to the intrinsic variation of the primary, and the eclipse light curve. New radial-velocity observations are presented and used to compute parameters of a spectroscopic orbit. Frequency analysis of the radial-velocity residuals from the spectroscopic orbital solution fails to uncover periodic variations with amplitudes greater than 2 km s (1). A Rossiter-McLaughlin anomaly is detected from observations covering ingress. From archival photometric indices and the revised Hipparcos parallax, we derive the primary's effective temperature, surface gravity, bolometric correction and the luminosity. An analysis of a high signal-to-noise spectrogram yields the effective temperature and surface gravity in good agreement with the photometric values. From the same spectrogram, we determine the abundance of He, C, N, O, Ne, Mg, Al, Si, P, S, Cl and Fe. The eclipse light curve is solved by means of EBOP. For a range of mass of the primary, a value of mean density, very nearly independent of assumed mass, is computed from the parameters of the system. Contrary to a recent report, this value is approximately equal to the mean density obtained from the star's effective temperature and luminosity. Despite limited frequency resolution of the MOST data, we were able to recover the closely spaced SPB frequency quadruplet discovered from the ground in 2002-2004. The other two SPB terms seen from the ground were also recovered. Moreover, our analysis of the MOST data adds 15 low-amplitude SPB terms with frequencies ranging from 0.109 to 2.786 d(-1). C1 [Jerzykiewicz, M.; Niemczura, E.; Molenda-Zakowicz, J.] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland. [Lehmann, H.; Hartmann, M.; Hrudkova, M.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Dymitrov, W.; Fagas, M.; Kaminski, K.] Adam Mickiewicz Univ, Astron Observ Inst, Fac Phys, PL-60286 Poznan, Poland. [Guenther, D. B.; Weiss, W. W.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Hrudkova, M.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Canary Islands, Spain. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Kuschnig, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kuschnig, R.; Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Leto, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jerzykiewicz, M (reprint author), Uniwersytetu Wroclawskiego, Inst Astron, Kopernika 11, PL-51622 Wroclaw, Poland. EM mjerz@astro.uni.wroc.pl RI Leto, Giuseppe/N-3355-2015 OI Leto, Giuseppe/0000-0002-0040-5011 FU MNiSW grant [N N203 405139]; NCN grant [2011/01/B/St9/05448]; Wroclaw Centre for Networking and Supercomputing [214]; DFG [HA 3279/5-1]; Natural Sciences and Engineering Research Council (NSERC) of Canada; Fonds de recherche du Quebec (FQNRT) FX We are indebted to Dr Paul B. Etzel for providing the source code of his computer program EBOP and explanations and to Dr Jadwiga Daszynska-Daszkiewicz for computing the evolutionary tracks used in Section 8. MJ, EN and JM-.Z acknowledge support from MNiSW grant N N203 405139. EN acknowledges support from NCN grant 2011/01/B/St9/05448. Calculations have been partially carried out at the Wroclaw Centre for Networking and Supercomputing under grant No. 214. MHr acknowledges support from DFG grant HA 3279/5-1. WD thanks his students, Karolina Bakowska, Adrian Kruszewski, Krystian Kurzawa and Anna Przybyszewska for assisting in observations. DBG, JMM, AFJM and SMR acknowledge funding support of the Natural Sciences and Engineering Research Council (NSERC) of Canada. AFJM is also grateful for financial assistance from Fonds de recherche du Quebec (FQNRT). In this research, we have used the Aladin service, operated at CDS, Strasbourg, France, and the SAO/NASA Astrophysics Data System Abstract Service. NR 59 TC 2 Z9 2 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 2 BP 1032 EP 1045 DI 10.1093/mnras/stt522 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300015 ER PT J AU Paragi, Z van der Horst, AJ Belloni, T Miller-Jones, JCA Linford, J Taylor, G Yang, J Garrett, MA Granot, J Kouveliotou, C Kuulkers, E Wijers, RAMJ AF Paragi, Z. van der Horst, A. J. Belloni, T. Miller-Jones, J. C. A. Linford, J. Taylor, G. Yang, J. Garrett, M. A. Granot, J. Kouveliotou, C. Kuulkers, E. Wijers, R. A. M. J. TI VLBI observations of the shortest orbital period black hole binary, MAXI J1659-152 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: MAXI J1659-152; ISM: jets and outflows; X-rays: binaries ID X-RAY BINARIES; RADIO JET; RELATIVISTIC JETS; LOW/HARD STATE; GX 339-4; CANDIDATE; OUTBURST; CYGNUS-X-3; EMISSION; TRANSIENT AB The X-ray transient MAXI J1659-152 was discovered by Swift/Burst Alert Telescope and it was initially identified as a gamma-ray burst. Soon its Galactic origin and binary nature were established. There exists a wealth of multiwavelength monitoring data for this source, providing a great coverage of the full X-ray transition in this candidate black hole binary system. We obtained two epochs of European very long baseline interferometry (VLBI) Network (EVN) electronic-VLBI and four epochs of Very Long Baseline Array data of MAXI J1659-152 which show evidence for outflow in the early phases. The overall source properties (polarization, milliarcsecond-scale radio structure, flat radio spectrum) are described well with the presence of a compact jet in the system through the transition from the hard-intermediate to the soft X-ray spectral state. The apparent dependence of source size and the radio core position on the observed flux density (luminosity-dependent core shift) supports this interpretation as well. We see no evidence for major discrete ejecta during the outburst. For the source proper motion we derive 2 Sigma upper limits of 115 mu as d(-1) in right ascension, and 37 mu as d(-1) in declination, over a time baseline of 12 d. These correspond to velocities of 1400 and 440 km s(-1), respectively, assuming a source distance of similar to 7 kpc. C1 [Paragi, Z.; Yang, J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [van der Horst, A. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Belloni, T.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Linford, J.; Taylor, G.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Garrett, M. A.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Garrett, M. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 38512 USA. [Kuulkers, E.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, E-28691 Madrid, Spain. [Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands. RP Paragi, Z (reprint author), Joint Inst VLBI Europe, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. EM zparagi@jive.nl RI Miller-Jones, James/B-2411-2013; OI Miller-Jones, James/0000-0003-3124-2814; Wijers, Ralph/0000-0002-3101-1808 FU European Union [RI-261525]; Australian Research Council [DP120102393]; European Community [ITN 215212]; European national research council; Chinese national research council; South African national research council; Netherlands Foundation for Scientific Research FX We thank the anonymous referee for the constructive comments, which helped to improve our paper significantly. ZP thanks to Andrei Lobanov for discussions about the compact jet model. e-VLBI research infrastructure in Europe is supported by the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreement RI-261525 NEXPReS. JCAMJ acknowledges support from an Australian Research Council Discovery Grant (DP120102393). The EVN is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. The WSRT is operated by Netherlands Institute for Radio Astronomy (ASTRON) with support from the Netherlands Foundation for Scientific Research. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work made use of the Swinburne University of Technology software correlator, developed as part of the Australian Major National Research Facilities Programme and operated under license. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement ITN 215212. NR 55 TC 9 Z9 9 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 2 BP 1319 EP 1329 DI 10.1093/mnras/stt545 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300036 ER PT J AU Foster, DL Charles, PA Swartz, DA Misra, R Stassun, KG AF Foster, D. L. Charles, P. A. Swartz, D. A. Misra, R. Stassun, K. G. TI Monitoring the very-long-term variability of X-ray sources in the giant elliptical galaxy M87 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; X-rays: binaries ID HUBBLE-SPACE-TELESCOPE; MASS BLACK-HOLE; NGC 5408 X-1; PERIODIC MODULATION; GLOBULAR-CLUSTERS; SPECTRAL-ANALYSIS; CENTRAL REGION; CHANDRA; M31; SUPERSOFT AB We report on our search for very-long-term variability (weeks to years) in X-ray binaries (XRBs) in the giant elliptical galaxy M87. We have used archival Chandra imaging observations to characterize the long-term variability of eight of the brightest members of the XRB population in M87. The peak brightness of some of the sources exceeded the ultraluminous X-ray source (ULXs) threshold luminosity of similar to 10(39) erg s(-1), and one source could exhibit dips or eclipses. We show that for one source, if it has similar modulation amplitude as in SS433, then period recoverability analysis on the current data would detect periodic modulations, but only for a narrow range of periods less than 120 d. We conclude that a dedicated monitoring campaign, with appropriately defined sampling, is essential if we are to investigate properly the nature of the long-term modulations such as those seen in Galactic sources. C1 [Foster, D. L.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Foster, D. L.; Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Charles, P. A.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Swartz, D. A.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35805 USA. [Misra, R.] Inter Univ Ctr Astron & Astrophys, Pune, Maharashtra, India. [Stassun, K. G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. RP Foster, DL (reprint author), S African Astron Observ, POB 9, ZA-7935 Observatory, South Africa. EM deatrick@saao.ac.za FU NASA; Vanderbilt-Cape Town Partnership Program; Astrophysics, Cosmology & Gravity Centre (ACGC) at the University of Cape Town; International Academic Programmes Office (IAPO) at the University of Cape Town FX DLF acknowledges support from NASA in the form of a Harriett G. Jenkins Fellowship; the Vanderbilt-Cape Town Partnership Program; the Astrophysics, Cosmology & Gravity Centre (ACGC) at the University of Cape Town; and the International Academic Programmes Office (IAPO) at the University of Cape Town. NR 35 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 2 BP 1375 EP 1381 DI 10.1093/mnras/stt557 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300042 ER PT J AU Martin, RG Lubow, SH AF Martin, Rebecca G. Lubow, Stephen H. TI Propagation of the gravo-magneto disc instability SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; planets and satellites: formation; protoplanetary discs; stars: pre-main-sequence ID LONG-TERM EVOLUTION; I PLANET MIGRATION; T TAURI DISKS; PROTOSTELLAR DISKS; DEAD ZONES; MAGNETOROTATIONAL-INSTABILITY; ACCRETION DISK; PROTOPLANETARY DISCS; EPISODIC ACCRETION; LAYERED ACCRETION AB Discs that contain dead zones are subject to the gravo-magneto instability which arises when the turbulence shifts from gravitational to magnetic. We have previously described this instability through a local analysis at some radius in the disc in terms of a limit cycle. A disc may be locally unstable over a radial interval. In this paper, we consider how the local instability model can describe global disc outbursts. The outburst is triggered near the middle of the range of locally unstable radii. The sudden increase in turbulence within high surface density material causes a snowplough of density that propagates both inwards and outwards. All radii inside the trigger radius become unstable, as well as locally unstable radii outside the trigger radius. In addition, a locally stable region outside the trigger radius may also become unstable as the gravitational instability is enhanced by the snowplough. For the circumstellar disc model we consider, we find that a quarter of the disc mass is accreted on to the central object during the outburst. The radius out to which the disc is globally unstable is twice that for which it is locally unstable. C1 [Martin, Rebecca G.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Lubow, Stephen H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Martin, RG (reprint author), NASA, Washington, DC 20546 USA. EM rebecca.martin@jila.colorado.edu FU California Institute of Technology (Caltech); NASA [NNX11AK61G] FX We thank the anonymous referee for useful comments. RGM acknowledges support provided in part through a contract with the California Institute of Technology (Caltech), funded by NASA, under the Sagan Fellowship Program. SHL acknowledges support from NASA grant NNX11AK61G. NR 43 TC 12 Z9 12 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 2 BP 1616 EP 1622 DI 10.1093/mnras/stt580 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300058 ER PT J AU Barnes, J Dove, M Lahsen, M Mathews, A McElwee, P McIntosh, R Moore, F O'Reilly, J Orlove, B Puri, R Weise, H Yager, K AF Barnes, Jessica Dove, Michael Lahsen, Myanna Mathews, Andrew McElwee, Pamela McIntosh, Roderick Moore, Frances O'Reilly, Jessica Orlove, Ben Puri, Rajindra Weise, Harvey Yager, Karina TI Contribution of anthropology to the study of climate change SO NATURE CLIMATE CHANGE LA English DT Article ID COLLAPSE; DISINTEGRATION; CIVILIZATION; SCIENCE; WEST; EAST AB Understanding the challenge that climate change poses and crafting appropriate adaptation and mitigation mechanisms requires input from the breadth of the natural and social sciences. Anthropology's in-depth fieldwork methodology, long engagement in questions of society-environment interactions and broad, holistic view of society yields valuable insights into the science, impacts and policy of climate change. Yet the discipline's voice in climate change debates has remained a relatively marginal one until now. Here, we identify three key ways that anthropological research can enrich and deepen contemporary understandings of climate change. C1 [Barnes, Jessica; Dove, Michael] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Barnes, Jessica; Dove, Michael] Yale Climate & Energy Inst, New Haven, CT 06511 USA. [Lahsen, Myanna] Ctr Earth Syst Sci, Sao Jose Dos Campos, Brazil. [Mathews, Andrew] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [McElwee, Pamela] Rutgers State Univ, New Brunswick, NJ 07102 USA. [McIntosh, Roderick; Weise, Harvey] Yale Univ, New Haven, CT 06511 USA. [Moore, Frances] Stanford Univ, Stanford, CA 94305 USA. [O'Reilly, Jessica] St Johns Univ, Coll St Benedicts, St Joseph, MN 56374 USA. [Orlove, Ben] Columbia Univ, New York, NY 10027 USA. [Puri, Rajindra] Univ Kent, Canterbury CT2 7NZ, Kent, England. [Yager, Karina] NASA, Greenbelt, MD 20771 USA. RP Barnes, J (reprint author), Yale Univ, Sch Forestry & Environm Studies, 195 Prospect St, New Haven, CT 06511 USA. EM jessica.barnes@yale.edu RI Lahsen, Myanna/E-3697-2013; OI Puri, Rajindra/0000-0002-3442-8537; McElwee, Pamela/0000-0003-3525-9285 FU Yale Climate and Energy Institute; Edward J. and Dorothy Clarke Kempf Fund; MacMillan Center for International and Area Studies; Tropical Resources Institute at Yale FX Funding for the workshop discussion that informed this Perspective and for the writing of the Perspective was provided by the Yale Climate and Energy Institute, the Edward J. and Dorothy Clarke Kempf Fund, the MacMillan Center for International and Area Studies and the Tropical Resources Institute at Yale. NR 50 TC 34 Z9 34 U1 2 U2 61 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD JUN PY 2013 VL 3 IS 6 BP 541 EP 544 DI 10.1038/NCLIMATE1775 PG 4 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 174OX UT WOS:000321166400011 ER PT J AU Shindell, D Faluvegi, G Nazarenko, L Bowman, K Lamarque, JF Voulgarakis, A Schmidt, GA Pechony, O Ruedy, R AF Shindell, Drew Faluvegi, Greg Nazarenko, Larissa Bowman, Kevin Lamarque, Jean-Francois Voulgarakis, Apostolos Schmidt, Gavin A. Pechony, Olga Ruedy, Reto TI Attribution of historical ozone forcing to anthropogenic emissions SO NATURE CLIMATE CHANGE LA English DT Article ID CLIMATE; SYSTEM AB Anthropogenic ozone radiative forcing is traditionally separately attributed to tropospheric and stratospheric changes assuming that these have distinct causes(1). Using the interactive composition-climate model GISS-E2-R we find that this assumption is not justified. Our simulations show that changes in. emissions of tropospheric ozone precursors have substantial effects on ozone in both regions, as do anthropogenic halocarbon emissions. On the basis of our results, further simulations with the NCAR-CAM3.5 model(2), and published studies(3,4), we estimate industrial era (1850-2005) whole-atmosphere ozone forcing of similar to 0.5Wm(-2) due to anthropogenic tropospheric precursors and about -0.2 W m(-2) due to halocarbons. The net troposphere plus stratosphere forcing is similar to the net halocarbon plus precursor ozone forcing, but the latter provides a more useful perspective. The halocarbon-induced ozone forcing is roughly two-thirds the magnitude of the halocarbon direct forcing but opposite in sign, yielding a net forcing of only similar to 0.1 W m(-2). Thus, the net effect of halocarbons has been smaller, and the effect of tropospheric ozone precursors has been greater, than generally recognized. C1 [Shindell, Drew; Faluvegi, Greg; Nazarenko, Larissa; Voulgarakis, Apostolos; Schmidt, Gavin A.; Pechony, Olga; Ruedy, Reto] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Shindell, Drew; Faluvegi, Greg; Nazarenko, Larissa; Voulgarakis, Apostolos; Schmidt, Gavin A.; Pechony, Olga; Ruedy, Reto] Columbia Univ, New York, NY 10025 USA. [Bowman, Kevin] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Lamarque, Jean-Francois] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Shindell, D (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM drew.t.shindell@nasa.gov RI Schmidt, Gavin/D-4427-2012; Shindell, Drew/D-4636-2012; Lamarque, Jean-Francois/L-2313-2014 OI Schmidt, Gavin/0000-0002-2258-0486; Lamarque, Jean-Francois/0000-0002-4225-5074 FU NASA MAP FX We thank NASA MAP for financial support and the NCCS for computer services. NR 20 TC 13 Z9 13 U1 1 U2 18 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD JUN PY 2013 VL 3 IS 6 BP 567 EP 570 DI 10.1038/NCLIMATE1835 PG 4 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 174OX UT WOS:000321166400016 ER PT J AU Xu, L Myneni, RB Chapin, FS Callaghan, TV Pinzon, JE Tucker, CJ Zhu, Z Bi, J Ciais, P Tommervik, H Euskirchen, ES Forbes, BC Piao, SL Anderson, BT Ganguly, S Nemani, RR Goetz, SJ Beck, PSA Bunn, AG Cao, C Stroeve, JC AF Xu, L. Myneni, R. B. Chapin, F. S., III Callaghan, T. V. Pinzon, J. E. Tucker, C. J. Zhu, Z. Bi, J. Ciais, P. Tommervik, H. Euskirchen, E. S. Forbes, B. C. Piao, S. L. Anderson, B. T. Ganguly, S. Nemani, R. R. Goetz, S. J. Beck, P. S. A. Bunn, A. G. Cao, C. Stroeve, J. C. TI Temperature and vegetation seasonality diminishment over northern lands SO NATURE CLIMATE CHANGE LA English DT Article ID ARCTIC VEGETATION; TUNDRA; ECOSYSTEMS; PLANT; DYNAMICS AB Global temperature is increasing, especially over northern lands (>50 degrees N), owing to positive feedbacks(1). As this increase is most pronounced in winter, temperature seasonality (S-T)-conventionally defined as the difference between summer and winter temperatures-is diminishing over time(2), a phenomenon that is analogous to its equatorward decline at an annual scale. The initiation, termination and performance of vegetation photosynthetic activity are tied to threshold temperatures(3). Trends in the timing of these thresholds and cumulative temperatures above them may alter vegetation productivity, or modify vegetation seasonality (S-V), over time. The relationship between S-T and S-V is critically examined here with newly improved ground and satellite data sets. The observed diminishment of S-T and S-V, is equivalent to 4 degrees and 7 degrees (5 degrees and 6 degrees) latitudinal shift equatorward during the past 30 years in the Arctic. (boreal) region. Analysis of simulations from 17 state-of-the-art climate models(4) indicates an additional S-T diminishment equivalent to a 20 equatorward shift could occur this century. How S-V will change in response to such large projected S-T declines and the impact this will have on ecosystem services(5) are not well understood. Hence the need for continued monitoring(6) of northern lands as their seasonal temperature profiles evolve to resemble those further south. C1 [Xu, L.; Myneni, R. B.; Zhu, Z.; Bi, J.; Anderson, B. T.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Chapin, F. S., III; Euskirchen, E. S.] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA. [Callaghan, T. V.] Royal Swedish Acad Sci, S-10405 Stockholm, Sweden. [Callaghan, T. V.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Pinzon, J. E.; Tucker, C. J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Ciais, P.] UVSQ, CNRS, CEA, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. [Tommervik, H.] Norwegian Inst Nat Res, Fram High North Res Ctr Climate & Environm, N-9296 Tromso, Norway. [Forbes, B. C.] Univ Lapland, Arctic Ctr, FI-96101 Rovaniemi, Finland. [Piao, S. L.] Peking Univ, Dept Ecol, Beijing 100871, Peoples R China. [Piao, S. L.] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100085, Peoples R China. [Ganguly, S.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Nemani, R. R.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. [Goetz, S. J.; Beck, P. S. A.] Woods Hole Res Ctr, Falmouth, MA 02540 USA. [Bunn, A. G.] Western Washington Univ, Huxley Coll, Dept Environm Sci, Bellingham, WA 98225 USA. [Cao, C.] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, State Key Lab Remote Sensing Sci, Beijing 100101, Peoples R China. [Cao, C.] Univ Elect Sci & Technol China, Sch Resource & Environm, Chengdu 611731, Sichuan, Peoples R China. [Stroeve, J. C.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. RP Xu, L (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. EM xuliang@bu.edu; ranga.myneni@gmail.com RI Forbes, Bruce/L-4431-2013; ganguly, sangram/B-5108-2010; Myneni, Ranga/F-5129-2012; Goetz, Scott/A-3393-2015; Xu, Liang/D-1247-2013; Callaghan, Terens/N-7640-2014; OI Forbes, Bruce/0000-0002-4593-5083; Goetz, Scott/0000-0002-6326-4308; Chapin III, F Stuart/0000-0002-2558-9910 FU NASA Earth Science Division FX This work was financially supported by the NASA Earth Science Division. We thank CRU, NSIDC, NASA MODIS Project, CAVM team and the CMIP5 climate modelling groups (listed in Supplementary Table S7) for making their data available. The authors thank U. S. Bhatt, H. E. Epstein, G. R. North, M. K. Raynolds, A. R. Stine, G. Schmidt and D. A. Walker for their comments on various parts of this article. NR 30 TC 150 Z9 159 U1 33 U2 230 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD JUN PY 2013 VL 3 IS 6 BP 581 EP 586 DI 10.1038/NCLIMATE1836 PG 6 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 174OX UT WOS:000321166400019 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bikmaev, I Bohringer, H Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bourdin, H Brown, ML Brown, SD Burenin, R Burigana, C Cabella, P Cardoso, JF Carvalho, P Catalano, A Cayon, L Chiang, LY Chon, G Christensen, PR Churazov, E Clements, DL Colafrancesco, S Colombo, LPL Coulais, A Crill, BP Cuttaia, F Da Silva, A Dahle, H Danese, L Davis, RJ de Bernardis, P de Gasperis, G de Rosa, A de Zotti, G Delabrouille, J Democles, J Desert, FX Dickinson, C Diego, JM Dolag, K Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Ensslin, TA Eriksen, HK Finelli, F Flores-Cacho, I Forni, O Frailis, M Franceschi, E Frommert, M Galeotta, S Ganga, K Genova-Santos, RT Giard, M Gilfanov, M Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Hansen, FK Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, TR Jagemann, T Jones, WC Juvela, M Keihanen, E Khamitov, I Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lawrence, CR Le Jeune, M Leonardi, R Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marleau, F Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Mei, S Melchiorri, A Melin, JB Mendes, L Mennella, A Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Munshi, D Murphy, JA Naselsky, P Natoli, P Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Pajot, F Paoletti, D Perdereau, O Perrotta, F Piacentini, F Piat, M Pierpaoli, E Piffaretti, R Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Roman, M Rosset, C Rossetti, M Rubino-Martin, JA Rudnick, L Rusholme, B Sandri, M Savini, G Schaefer, BM Scott, D Smoot, GF Stivoli, F Sudiwala, R Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tuovinen, J Turler, M Umana, G Valenziano, L Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Welikala, N White, SDM Yvon, D Zacchei, A Zaroubi, S Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bikmaev, I. Boehringer, H. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bourdin, H. Brown, M. L. Brown, S. D. Burenin, R. Burigana, C. Cabella, P. Cardoso, J. -F. Carvalho, P. Catalano, A. Cayon, L. Chiang, L. -Y Chon, G. Christensen, P. R. Churazov, E. Clements, D. L. Colafrancesco, S. Colombo, L. P. L. Coulais, A. Crill, B. P. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. Davis, R. J. de Bernardis, P. de Gasperis, G. de Rosa, A. de Zotti, G. Delabrouille, J. Democles, J. Desert, F. -X. Dickinson, C. Diego, J. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Ensslin, T. A. Eriksen, H. K. Finelli, F. Flores-Cacho, I. Forni, O. Frailis, M. Franceschi, E. Frommert, M. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Gilfanov, M. Gonzalez-Nuevo, J. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Henrot-Versille, S. Hernandez-Monteagudo, C. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, T. R. Jagemann, T. Jones, W. C. Juvela, M. Keihanen, E. Khamitov, I. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lawrence, C. R. Le Jeune, M. Leonardi, R. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marleau, F. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Mei, S. Melchiorri, A. Melin, J. -B. Mendes, L. Mennella, A. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Munshi, D. Murphy, J. A. Naselsky, P. Natoli, P. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Pajot, F. Paoletti, D. Perdereau, O. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Piffaretti, R. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Roman, M. Rosset, C. Rossetti, M. Rubino-Martin, J. A. Rudnick, L. Rusholme, B. Sandri, M. Savini, G. Schaefer, B. M. Scott, D. Smoot, G. F. Stivoli, F. Sudiwala, R. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tuovinen, J. Tuerler, M. Umana, G. Valenziano, L. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Welikala, N. White, S. D. M. Yvon, D. Zacchei, A. Zaroubi, S. Zonca, A. CA Planck Collaboration TI Planck intermediate results X. Physics of the hot gas in the Coma cluster SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: Coma cluster; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters; cosmology: observations; galaxies: clusters: general; cosmic background radiation ID LARGE-SCALE STRUCTURE; PRE-LAUNCH STATUS; SIMULATED GALAXY CLUSTERS; ALL-SKY SURVEY; SUNYAEV-ZELDOVICH; RADIO HALOS; XMM-NEWTON; SHOCK-WAVES; MAGNETIC-FIELD; TEMPERATURE STRUCTURE AB We present an analysis of Planck satellite data on the Coma cluster observed via the Sunyaev-Zeldovich effect. Thanks to its great sensitivity, Planck is able, for the first time, to detect SZ emission up to r approximate to 3 x R-500. We test previously proposed spherically symmetric models for the pressure distribution in clusters against the azimuthally averaged data. In particular, we find that the Arnaud et al. (2010, A&A, 517, A92) "universal" pressure profile does not fit Coma, and that their pressure profile for merging systems provides a reasonable fit to the data only at r < R-500; by r = 2 x R-500 it underestimates the observed y profile by a factor of similar or equal to 2. This may indicate that at these larger radii either: i) the cluster SZ emission is contaminated by unresolved SZ sources along the line of sight; or ii) the pressure profile of Coma is higher at r > R-500 than the mean pressure profile predicted by the simulations used to constrain the models. The Planck image shows significant local steepening of the y profile in two regions about half a degree to the west and to the south-east of the cluster centre. These features are consistent with the presence of shock fronts at these radii, and indeed the western feature was previously noticed in the ROSAT PSPC mosaic as well as in the radio. Using Planck y profiles extracted from corresponding sectors we find pressure jumps of 4.9(-0.2)(+0.4) and 5.0(-0.1)(+1.3) in the west and south-east, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number M-w = 2.03(-0.04)(+0.09) and M-se = 2.05(-0.02)(+0.25) in the west and south-east, respectively. Finally, we find that the y and radio-synchrotron signals are quasi-linearly correlated on Mpc scales, with small intrinsic scatter. This implies either that the energy density of cosmic-ray electrons is relatively constant throughout the cluster, or that the magnetic fields fall off much more slowly with radius than previously thought. C1 [Bartlett, J. G.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Le Jeune, M.; Piat, M.; Remazeilles, M.; Roman, M.; Rosset, C.; Smoot, G. F.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu, F-75205 Paris 13, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Bikmaev, I.] Acad Sci Tatarstan, Kazan 420111, Russia. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Ashdown, M.; Carvalho, P.; Hobson, M.; Lasenby, A.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Kneissl, R.] ALMA Santiago Cent Offices, Atacama Large Millimeter Submillimeter Array, Santiago 7630355, Chile. [Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Flores-Cacho, I.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Dore, O.; Hildebrandt, S. R.; Mei, S.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Dahle, H.; Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway. [Da Silva, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [Borrill, J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Rebolo, R.] CSIC, Madrid, Spain. [Melin, J. -B.; Piffaretti, R.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Frommert, M.; Kunz, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva, Switzerland. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Bikmaev, I.] Kazan Fed Univ, Dept Astron & Geodesy, Kazan 420008, Russia. [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA. [Brown, S. D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Cayon, L.] Purdue Univ, Dept Stat, W Lafayette, IN 47907 USA. [Matarrese, S.] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Burigana, C.; Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Balbi, A.; Bourdin, H.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, Rome, Italy. [Cabella, P.] Univ Roma Tor Vergata, Dipartimento Matemat, Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago 19001, Chile. [Dupac, X.; Jagemann, T.; Leonardi, R.; Mendes, L.] Planck Sci Off, ESAC, European Space Agcy, Madrid, Spain. [Tauber, J. A.] Estec, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Mei, S.] Observ Paris, Sect Meudon, GEPI, F-92195 Meudon, France. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy. [de Zotti, G.] Osserv Astrofis Catania, INAF, I-35131 Padua, Italy. [Colafrancesco, S.; Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Massardi, M.] CNR, Ist Radioastron, INAF, I-40126 Bologna, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Melchiorri, A.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy. [Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France. [Desert, F. -X.; Ponthieu, N.] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Tuerler, M.] Univ Geneva, ISDC Data Ctr Astrophys, Versoix, Switzerland. [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India. [Clements, D. L.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, Inst Neel, CNRS, F-38041 Grenoble, France. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Balbi, A.; Benoit, A.; Bonaldi, A.; Dole, H.; Douspis, M.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.; Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, CNRS UMR 8617, Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest, Romania. [Marleau, F.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Harrison, D.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Dahle, H.; Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Diego, J. M.; Gonzalez-Nuevo, J.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Rocha, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bonaldi, A.; Brown, M. L.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Zaroubi, S.] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [Ashdown, M.; Harrison, D.; Lasenby, A.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS IN2P3, LAL, Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Democles, J.; Piffaretti, R.; Pratt, G. W.] Univ Paris Diderot, CNRS, Lab AIM, IRFU Serv Astrophys,CEA,DSM,CEA Saclay, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Hurier, G.; Macias-Perez, J. F.; Renault, C.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Churazov, E.; Dolag, K.; Doerl, U.; Ensslin, T. A.; Gilfanov, M.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Boehringer, H.; Chon, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland. [Rudnick, L.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Burenin, R.] Space Res Inst IKI, Moscow, Russia. [Churazov, E.; Gilfanov, M.; Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Khamitov, I.] Akdeniz Univ Campus, TUBITAK Natl Observ, TR-07058 Antalya, Turkey. [Benabed, K.; Bouchet, F. R.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UPMC, UMR7095, F-75014 Paris, France. [Schaefer, B. M.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Mei, S.] Univ Paris 07, F-75205 Paris 13, France. [Banday, A. J.; Flores-Cacho, I.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, IRAP, UPS OMP, F-31028 Toulouse 4, France. [Dolag, K.] Univ Munich, Univ Observ, D-81679 Munich, Germany. [Battaner, E.] Univ Granada, Dept Fis Teor & Cosmos, Fac Ciencias, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Mazzotta, P (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, Rome, Italy. EM mazzotta@roma2.infn.it RI Remazeilles, Mathieu/N-1793-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Mazzotta, Pasquale/B-1225-2016; Battaner, Eduardo/P-7019-2014; de Gasperis, Giancarlo/C-8534-2012; Lopez-Caniego, Marcos/M-4695-2013; Da Silva, Antonio/A-2693-2010; Bouchet, Francois/B-5202-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Churazov, Eugene/A-7783-2013; Gonzalez-Nuevo, Joaquin/I-3562-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014 OI Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Pierpaoli, Elena/0000-0002-7957-8993; TERENZI, LUCA/0000-0001-9915-6379; Hurier, Guillaume/0000-0002-1215-0706; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; de Gasperis, Giancarlo/0000-0003-2899-2171; Da Silva, Antonio/0000-0002-6385-1609; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (Spain); JA (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU); U.S. NSF [09-08668] FX A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/Planck_Collaboration. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). Partial support for this work for L. Rudnick comes from U.S. NSF Grant 09-08668 to the University of Minnesota. We would also like to acknowledge useful conversations with G. Brunetti. NR 94 TC 23 Z9 23 U1 1 U2 32 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2013 VL 554 AR A140 DI 10.1051/0004-6361/201220247 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200138 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Balbi, A Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Bernard, JP Bersanelli, M Bonaldi, A Bond, JR Borrill, J Bouchet, FR Burigana, C Cabella, P Cardoso, JF Catalano, A Cayon, L Chary, RR Chiang, LY Christensen, PR Clements, DL Colombo, LPL Coulais, A Crill, BP Cuttaia, F Danese, L D'Arcangelo, O Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Dickinson, C Diego, JM Dobler, G Dole, H Donzelli, S Dore, O Dorl, U Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Gonzaalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Hildebrandt, SR Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, TR Jagemann, T Jewell, J Jones, WC Juvela, M Keihacn, E Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lawrence, CR Leach, S Leonardi, R Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Mitra, S Moneti, A Montier, L Morgante, G Munshi, D Murphy, JA Naselsky, P Natoli, P Norgaard-Nielsen, HU Noviello, F Novikov, D Osborne, S Pajot, F Paladini, R Paoletti, D Partridge, B Pearson, TJ Perdereau, O Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Sandri, M Savini, G Schaefer, BM Scott, D Smoot, GF Spencer, L Stivoli, F Sudiwala, R Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Turler, M Umana, G Valenziano, L Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, M Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Balbi, A. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Bernard, J. -P. Bersanelli, M. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Burigana, C. Cabella, P. Cardoso, J. -F. Catalano, A. Cayon, L. Chary, R. -R. Chiang, L. -Y. Christensen, P. R. Clements, D. L. Colombo, L. P. L. Coulais, A. Crill, B. P. Cuttaia, F. Danese, L. D'Arcangelo, O. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Dickinson, C. Diego, J. M. Dobler, G. Dole, H. Donzelli, S. Dore, O. Doerl, U. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Hildebrandt, S. R. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, T. R. Jagemann, T. Jewell, J. Jones, W. C. Juvela, M. Keihaecn, E. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lawrence, C. R. Leach, S. Leonardi, R. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Mitra, S. Moneti, A. Montier, L. Morgante, G. Munshi, D. Murphy, J. A. Naselsky, P. Natoli, P. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Osborne, S. Pajot, F. Paladini, R. Paoletti, D. Partridge, B. Pearson, T. J. Perdereau, O. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savini, G. Schaefer, B. M. Scott, D. Smoot, G. F. Spencer, L. Stivoli, F. Sudiwala, R. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tuerler, M. Umana, G. Valenziano, L. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results IX. Detection of the Galactic haze with Planck SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy: nucleus; ISM: structure; ISM: bubbles; radio continuum: ISM ID MICROWAVE-ANISOTROPY-PROBE; PRE-LAUNCH STATUS; BAYESIAN COMPONENT SEPARATION; INTERSTELLAR-MEDIUM EMISSION; POWER SPECTRUM ESTIMATION; SPINNING DUST GRAINS; WMAP OBSERVATIONS; FOREGROUND EMISSION; TEMPERATURE DATA; NORTHERN SKY AB Using precise full-sky observations from Planck, and applying several methods of component separation, we identify and characterise the emission from the Galactic "haze" at microwave wavelengths. The haze is a distinct component of diffuse Galactic emission, roughly centered on the Galactic centre, and extends to vertical bar b vertical bar similar to 35-50 degrees in Galactic latitude and vertical bar l vertical bar similar to 15-20 degrees in longitude. By combining the Planck data with observations from the Wilkinson Microwave Anisotropy Probe, we were able to determine the spectrum of this emission to high accuracy, unhindered by the strong systematic biases present in previous analyses. The derived spectrum is consistent with power-law emission with a spectral index of -2.56 +/- 0.05, thus excluding free-free emission as the source and instead favouring hard-spectrum synchrotron radiation from an electron population with a spectrum (number density per energy) dN/dE proportional to E-2.1. At Galactic latitudes vertical bar b vertical bar < 30 degrees, the microwave haze morphology is consistent with that of the Fermi gamma-ray "haze" or "bubbles", while at b similar to -50 degrees we have identified an edge in the microwave haze that is spatially coincident with the edge in the gamma-ray bubbles. Taken together, this indicates that we have a multi-wavelength view of a distinct component of our Galaxy. Given both the very hard spectrum and the extended nature of the emission, it is highly unlikely that the haze electrons result from supernova shocks in the Galactic disk. Instead, a new astrophysical mechanism for cosmic-ray acceleration in the inner Galaxy is implied. C1 [Bartlett, J. G.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris Diderot, Sorbonne Paris Cite, APC, CNRS IN2P3,CEA Irfu,Observ Paris, F-75205 Paris 13, France. [Lahteenmaki, A.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, Cape Town, South Africa. [Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Ashdown, M.; Hobson, M.; Lasenby, A.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bond, J. R.; Martin, P. G.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Dore, O.; Helou, G.; Hildebrandt, S. R.; Pearson, T. J.] CALTECH, Pasadena, CA 91125 USA. [Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [Borrill, J.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA USA. [Rebolo, R.] CSIC, Madrid, Spain. [Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Kunz, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dana & David Dornsife Coll Letter,Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Juvela, M.; Keihaecn, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Smoot, G. F.; White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Cayon, L.; Mendes, L.] Purdue Univ, Dept Stat, W Lafayette, IN 47907 USA. [Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Balbi, A.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Cabella, P.] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] ULL, Dpto Astrofis, Tenerife 38206, Spain. [Dupac, X.; Jagemann, T.; Leonardi, R.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Giardino, G.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland. [Umana, G.] INAF Osserv Astrofis Catania, Catania, Italy. INAF Osserv Astron Padova, Padua, Italy. [Polenta, G.] INAF Osserv Astron Roma, Monte Porzio Catone, Italy. [de Zotti, G.; Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Zacchei, A.] INAF Osserv Astron Trieste, Trieste, Italy. [Massardi, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Melchiorri, A.] Univ Roma La Sapienza, Sez Roma 1, INFN, I-00185 Rome, Italy. [Stivoli, F.] Univ Paris 11, Lab Rech Informat, INRIA, F-91405 Orsay, France. [Ponthieu, N.] Univ Grenoble 1, CNRS INSU, UMR 5274, IPAG, F-38041 Grenoble, France. [Tuerler, M.] Univ Geneva, ISDC Data Ctr Astrophys, Versoix, Switzerland. [Mitra, S.] Pune Univ Campus, IUCAA, Pune 411007, Maharashtra, India. [Clements, D. L.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Chary, R. -R.; Paladini, R.; Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Dole, H.; Douspis, M.; Kunz, M.; Lagache, G.; Pajot, F.; Ponthieu, N.; Puget, J. -L.] Univ Paris 11, UMR 8617, CNRS, Inst Astrophys Spatiale, Orsay, France. [Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest, Romania. [Chiang, L. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Efstathiou, G.; Gratton, S.; Harrison, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Diego, J. M.; Gonzalez-Nuevo, J.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, Santander, Spain. [D'Arcangelo, O.] CNR ENEA EURATOM Assoc, Ist Fis Plasma, Milan, Italy. [Bonaldi, A.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Gratton, S.; Harrison, D.; Lasenby, A.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Dobler, G.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS IN2P3, LAL, Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Marshall, D. J.; Pratt, G. W.] Univ Paris Diderot, CEA Saclay, CEA DSM, Lab AIM,IRFU Serv Astrophys,CNRS, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Macias-Perez, J. F.; Renault, C.] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS IN2P3, Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Lab Phys Theor, CNRS, F-91405 Orsay, France. [Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Doerl, U.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Pasadena, CA 36717 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Benabed, K.; Bouchet, F. R.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, F-75014 Paris, France. [Schaefer, B. M.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Banday, A. J.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Gorski, KM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM krzysztof.m.gorski@jpl.nasa.gov RI Lopez-Caniego, Marcos/M-4695-2013; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Bouchet, Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Novikov, Dmitry/P-1807-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Colombo, Loris/J-2415-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Mazzotta, Pasquale/B-1225-2016; OI Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Pierpaoli, Elena/0000-0002-7957-8993; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; WANDELT, Benjamin/0000-0002-5854-8269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Mazzotta, Pasquale/0000-0002-5411-1748; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Finelli, Fabio/0000-0002-6694-3269; De Zotti, Gianfranco/0000-0003-2868-2595 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (Spain); JA (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU); National Aeronautics and Space Administration; Harvey L. Karp Discovery Award FX The development of Planck has been supported by ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/Planck. Part of the research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. G. Dobler has been supported by the Harvey L. Karp Discovery Award. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. NR 69 TC 30 Z9 30 U1 1 U2 24 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 JUN PY 2013 VL 554 AR A139 DI 10.1051/0004-6361/201220271 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200137 ER PT J AU Burgarella, D Buat, V Gruppioni, C Cucciati, O Heinis, S Berta, S Bethermin, M Bock, J Cooray, A Dunlop, JS Farrah, D Franceschini, A Le Floc'h, E Lutz, D Magnelli, B Nordon, R Oliver, SJ Page, MJ Popesso, P Pozzi, F Riguccini, L Vaccari, M Viero, M AF Burgarella, D. Buat, V. Gruppioni, C. Cucciati, O. Heinis, S. Berta, S. Bethermin, M. Bock, J. Cooray, A. Dunlop, J. S. Farrah, D. Franceschini, A. Le Floc'h, E. Lutz, D. Magnelli, B. Nordon, R. Oliver, S. J. Page, M. J. Popesso, P. Pozzi, F. Riguccini, L. Vaccari, M. Viero, M. TI Herschel PEP/HerMES: the redshift evolution (0 <= z <= 4) of dust attenuation and of the total (UV plus IR) star formation rate density SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE early Universe; cosmology: observations; galaxies: star formation; infrared: galaxies; galaxies: starburst; ultraviolet: galaxies ID LYMAN-BREAK GALAXIES; EARLY RELEASE SCIENCE; LUMINOSITY FUNCTION; FORMATION HISTORY; FORMING GALAXIES; DISTANT GALAXIES; GAS ACCRETION; STELLAR MASS; ULTRAVIOLET; MULTIWAVELENGTH AB Using new homogeneous luminosity functions (LFs) in the far-ultraviolet (FUV) from VVDS and in the far-infrared (FIR) from Herschel/PEP and Herschel/HerMES, we studied the evolution of the dust attenuation with redshift. With this information, we were able to estimate the redshift evolution of the total (FUV + FIR) star formation rate density (SFRDTOT). By integrating SFRDTOT, we followed the mass building and analyzed the redshift evolution of the stellar mass density (SMD). This article aims at providing a complete view of star formation from the local Universe to z similar to 4 and, using assumptions on earlier star formation history, compares this evolution with previously published data in an attempt to draw a homogeneous picture of the global evolution of star formation in galaxies. Our main conclusions are that: 1) the dust attenuation A(FUV) is found to increase from z = 0 to z similar to 1.2 and then starts to decrease until our last data point at z = 3 : 6; 2) the estimated SFRD confirms published results to z similar to 2. At z > 2, we observe either a plateau or a small increase up to z similar to 3 and then a likely decrease up to z = 3.6; 3) the peak of AFUV is delayed with respect to the plateau of SFRDTOT and a probable origin might be found in the evolution of the bright ends of the FUV and FIR LFs; 4) using assumptions (exponential rise and linear rise with time) for the evolution of the star formation density from z = 3 : 6 to z(form) = 10, we integrated SFRDTOT and obtained a good agreement with the published SMDs. C1 [Burgarella, D.; Buat, V.; Heinis, S.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Gruppioni, C.; Cucciati, O.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Berta, S.; Lutz, D.; Magnelli, B.; Nordon, R.; Popesso, P.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Bethermin, M.; Le Floc'h, E.; Riguccini, L.] Univ Paris Diderot, CNRS, CEA DSM Irfu, Lab AIM Paris Saclay,CE Saclay, F-91191 Gif Sur Yvette, France. [Bock, J.; Cooray, A.; Viero, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dunlop, J. S.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Farrah, D.; Oliver, S. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Franceschini, A.; Vaccari, M.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pozzi, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Vaccari, M.] Univ Western Cape, Astrophys Grp, Dept Phys, ZA-7535 Cape Town, South Africa. RP Burgarella, D (reprint author), Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. EM denis.burgarella@oamp.fr RI Vaccari, Mattia/R-3431-2016 OI Vaccari, Mattia/0000-0002-6748-0577 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); PRIN-INAF [1.06.09.05]; ASI-INAF [I00507/1, I005110]; Stockholm Observatory (Sweden) FX PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The authors acknowledge financial contribution from the contracts PRIN-INAF 1.06.09.05 and ASI-INAF I00507/1 and I005110. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, OAMP (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); and Caltech/JPL, IPAC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM; http://hedam.oamp.fr/HerMES). This work makes use of TOPCAT (http://www.star.bristol.ac.uk/?mbt/topcat/). NR 59 TC 33 Z9 33 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2013 VL 554 AR A70 DI 10.1051/0004-6361/201321651 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200069 ER PT J AU Daemgen, S Petr-Gotzens, MG Correia, S Teixeira, PS Brandner, W Kley, W Zinnecker, H AF Daemgen, S. Petr-Gotzens, M. G. Correia, S. Teixeira, P. S. Brandner, W. Kley, W. Zinnecker, H. TI Protoplanetary disk evolution and stellar parameters of T Tauri binaries in Chamaeleon I SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: late-type; stars: formation; circumstellar matter; binaries: visual ID STAR-FORMING REGION; MAIN-SEQUENCE STARS; LOW-MASS STARS; SUBMILLIMETER CONTINUUM FLUX; ORION NEBULA CLUSTER; CIRCUMSTELLAR DISKS; YOUNG BINARIES; SPECTROSCOPIC SURVEY; MULTIPLE SYSTEMS; MOLECULAR CLOUD AB Aims: This study aims to determine the impact of stellar binary companions on the lifetime and evolution of circumstellar disks in the Chamaeleon I (Cha I) star-forming region by measuring the frequency and strength of accretion and circumstellar dust signatures around the individual components of T Tauri binary stars. Methods. We used high-angular resolution adaptive optics JHK(s)L'-band photometry and 1.5-2.5 mu m spectroscopy of 19 visual binary and 7 triple stars in Cha I - including one newly discovered tertiary component - with separations between similar to 25 and similar to 1000 AU. The data allowed us to infer stellar component masses and ages and, from the detection of near-infrared excess emission and the strength of Brackett-gamma emission, the presence of ongoing accretion and hot circumstellar dust of the individual stellar components of each binary. Results. Of all the stellar components in close binaries with separations of 25-100 AU, 10(-5)(+15)% show signs of accretion. This is less than half of the accretor fraction found in wider binaries, which itself appears significantly reduced (similar to 44%) compared with previous measurements of single stars in Cha I. Hot dust was found around 50(-15)(+30)% of the target components, a value that is indistinguishable from that of Cha I single stars. Only the closest binaries (<25 AU) were inferred to have a significantly reduced fraction (less than or similar to 25%) of components that harbor hot dust. Accretors were exclusively found in binary systems with unequal component masses M-secondary/M-primary < 0.8, implying that the detected accelerated disk dispersal is a function of mass-ratio. This agrees with the finding that only one accreting secondary star was found, which is also the weakest accretor in the sample. Conclusions. The results imply that disk dispersal is more accelerated the stronger the dynamical disk truncation, i.e., the smaller the inferred radius of the disk. Nonetheless, the overall measured mass accretion rates appear to be independent of the cluster environment or the existence of stellar companions at any separation greater than or similar to 25 AU, because they agree well with observations from our previous binary study in the Orion Nebula cluster and with studies of single stars in these and other star-forming regions. C1 [Daemgen, S.; Petr-Gotzens, M. G.] European So Observ, D-85748 Garching, Germany. [Daemgen, S.] Univ Toronto, Dept Astron Astrophys, Toronto, ON M5S 3H4, Canada. [Correia, S.] Univ Hawaii, Inst Astron, Pukalani, HI 96768 USA. [Teixeira, P. S.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Brandner, W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kley, W.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Zinnecker, H.] NASA Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Zinnecker, H.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. RP Daemgen, S (reprint author), European So Observ, Karl Schwarzschildstr 2, D-85748 Garching, Germany. EM daemgen@astro.utoronto.ca RI Teixeira, Paula Stella/O-2289-2013; Kley, Wilhelm/A-4921-2012; OI Teixeira, Paula Stella/0000-0002-3665-5784; Daemgen, Sebastian/0000-0001-9915-2132 FU National Aeronautics and Space Administration; National Science Foundation; Austrian Science Fund (FWF) FX We thank the anonymous referee for a thoughtful report. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. It has used data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication is supported by the Austrian Science Fund (FWF). NR 75 TC 13 Z9 13 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 JUN PY 2013 VL 554 AR A43 DI 10.1051/0004-6361/201321220 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200042 ER PT J AU Grinberg, V Hell, N Pottschmidt, K Bock, M Nowak, MA Rodriguez, J Bodaghee, A Bel, MC Case, GL Hanke, M Kuhnel, M Markoff, SB Pooley, GG Rothschild, RE Tomsick, JA Wilson-Hodge, CA Wilms, J AF Grinberg, V. Hell, N. Pottschmidt, K. Boeck, M. Nowak, M. A. Rodriguez, J. Bodaghee, A. Bel, M. Cadolle Case, G. L. Hanke, M. Kuehnel, M. Markoff, S. B. Pooley, G. G. Rothschild, R. E. Tomsick, J. A. Wilson-Hodge, C. A. Wilms, J. TI Long term variability of Cygnus X-1 V. State definitions with all sky monitors SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; stars: individual: Cygnus X-1; binaries: close ID RAY-TIMING-EXPLORER; GLAST BURST MONITOR; X-RAY; ORBITAL MODULATION; RADIO-EMISSION; HARD STATE; BINARIES; JET; EVOLUTION; SPECTROSCOPY AB We present a scheme for determining the spectral state of the canonical black hole Cyg X-1 using data from previous and current X-ray all sky monitors (RXTE-ASM, Swift-BAT, MAXI, and Fermi-GBM). Determinations of the hard/intermediate and soft state agree to better than 10% between different monitors, facilitating the determination of the state and its context for any observation of the source, potentially over the lifetimes of different individual monitors. A separation of the hard and the intermediate states, which strongly differ in their spectral shape and short-term timing behavior, is only possible when data in the soft X-rays (<5 keV) are available. A statistical analysis of the states confirms the different activity patterns of the source (e.g., month- to year-long hard-state periods or phases during which numerous transitions occur). It also shows that the hard and soft states are stable, with the probability of Cyg X-1 remaining in a given state for at least one week to be larger than 85% in the hard state and larger than 75% in the soft state. Intermediate states are short lived, with a 50% probability that the source leaves the intermediate state within three days. Reliable detection of these potentially short-lived events is only possible with monitor data that have a time resolution better than 1 d. C1 [Grinberg, V.; Hell, N.; Hanke, M.; Kuehnel, M.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany. [Hell, N.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Boeck, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Nowak, M. A.] MIT CXC, Cambridge, MA 02139 USA. [Rodriguez, J.] Univ Paris Diderot, Lab AIM, UMR 7158, IRFU SAp, F-91191 Gif Sur Yvette, France. [Bodaghee, A.; Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bel, M. Cadolle] European Space Astron Ctr ESA ESAC, Madrid 28691, Spain. [Grinberg, V.; Case, G. L.] La Sierra Univ, Dept Phys, Riverside, CA 92515 USA. [Kuehnel, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1058 SJ Amsterdam, Netherlands. [Pooley, G. G.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Rothschild, R. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Wilson-Hodge, C. A.] NASA Marshall Space Flight Ctr, ZP 12, Huntsville, AL 35812 USA. RP Grinberg, V (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany. EM victoria.grinberg@fau.de RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468 FU Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und Raumfahrt Grant [50OR1007, 50OR1113]; European Commission through "Black Hole Universe" [ITN 215212]; LLNL [DE-AC52-07NA27344]; NASA; Faculty of the European Space Astronomy Centre (ESAC) FX This work has been partially funded by the Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und Raumfahrt Grants 50OR1007 and 50OR1113 and by the European Commission through ITN 215212 "Black Hole Universe". It was partially completed by LLNL under Contract DE-AC52-07NA27344, and is supported by NASA grants to LLNL and NASA/GSFC. This research has made use of the MAXI data provided by RIKEN, JAXA and the MAXI team. We thank John E. Davis for the development of the slxfig module used to prepare all figures in this work. V.G. thanks NASA's Goddard Space Flight Center for its hospitality during the time when the research presented here was done. V.G. and M.C.B. acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). NR 53 TC 18 Z9 18 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2013 VL 554 AR A88 DI 10.1051/0004-6361/201321128 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200087 ER PT J AU Hacar, A Tafalla, M Kauffmann, J Kovacs, A AF Hacar, A. Tafalla, M. Kauffmann, J. Kovacs, A. TI Cores, filaments, and bundles: hierarchical core formation in the L1495/B213 Taurus region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; ISM: kinematics and dynamics; ISM: molecules; ISM: structure; stars: formation; radio lines: ISM ID DENSE CLOUD CORES; STAR-FORMATION; MOLECULAR CLOUD; DARK CLOUDS; INTERNAL STRUCTURE; INITIAL CONDITIONS; DUST CLOUDS; GOULD BELT; FRAGMENTATION; EVOLUTION AB Context. Core condensation is a critical step in the star-formation process, but it is still poorly characterized observationally. Aims. We have studied the 10 pc-long L1495/B213 complex in Taurus to investigate how dense cores have condensed out of the lower density cloud material. Methods. We observed L1495/B213 in (CO)-O-18(1-0), N2H+ (1-0), and SO(J(N) = 3(2)-2(1)) with the 14m FCRAO telescope, and complemented the data with dust continuum observations using APEX (870 mu m) and IRAM 30 m (1200 mu m). Results. From the N2H+ emission, we identify 19 dense cores, some starless and some protostellar. They are not distributed uniformly, but tend to cluster with relative separations on the order of 0.25 pc. From the (CO)-O-18 emission, we identify multiple velocity components in the gas. We have characterized them by fitting Gaussians to the spectra and by studying the distribution of the fits in position-position-velocity space. In this space, the (CO)-O-18 components appear as velocity-coherent structures, and we identify them automatically using a dedicated algorithm (FIVE: Friends In VElocity). Using this algorithm, we identify 35 filamentary components with typical lengths of 0.5 pc, sonic internal velocity dispersions, and mass-per-unit length close to the stability threshold of isothermal cylinders at 10 K. Core formation seems to have occurred inside the filamentary components via fragmentation, with few fertile components with higher mass-per-unit length being responsible for most cores in the cloud. On large scales, the filamentary components appear grouped into families, which we refer to as bundles. Conclusions. Core formation in L1495/B213 has proceeded by hierarchical fragmentation. The cloud fragmented first into several pc-scale regions. Each of these regions later fragmented into velocity-coherent filaments of about 0.5 pc in length. Finally, a small number of these filaments fragmented quasi-statically and produced the individual dense cores we see today. C1 [Hacar, A.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Hacar, A.] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [Kauffmann, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kovacs, A.] Univ Minnesota, Minneapolis, MN 55414 USA. RP Hacar, A (reprint author), Observ Astron Nacl IGN, Alfonso 12 3, Madrid 28014, Spain. EM alvaro.hacar@univie.ac.at RI Kovacs, Attila/C-1171-2010; OI Kovacs, Attila/0000-0001-8991-9088; Hacar, Alvaro/0000-0001-5397-6961 FU MINECO [CSD2009-00038]; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX We thank Mark Heyer for assistance during the FCRAO observations We thank Carlos De Breuck, Thomas Stanke, and Giorgio Siringo for assistance during the APEX observations, and Axel Weiss and Arnaud Belloche for help with the data reduction. We also thank Guillermo Quintana-Lacaci and the IRAM staff for help during the MAMBO observations. An anonymous referee provided a number of useful comments and suggestions that are greatly appreciated. This publication is supported by the Austrian Science Fund (FWF). This research made use of NASA's Astrophysics Data System Bibliographic Services and the SIMBAD database, operated at the CDS, Strasbourg, France. M.T. acknowledges support by MINECO within the program CONSOLIDER INGENIO 2010, under grant "Molecular Astrophysics: The Herschel and ALMA era - ASTROMOL" (ref.: CSD2009-00038).; Based on observations carried out with the FCRAO 14m and IRAM 30m telescopes. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). Also based on data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory (ESO projects 080.C-3054 and 083.C-0453). NR 77 TC 83 Z9 84 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 JUN PY 2013 VL 554 AR A55 DI 10.1051/0004-6361/201220090 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200054 ER PT J AU Pineda, JL Langer, WD Velusamy, T Goldsmith, PF AF Pineda, J. L. Langer, W. D. Velusamy, T. Goldsmith, P. F. TI A Herschel [C II] Galactic plane survey I. The global distribution of ISM gas components SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; stars: formation; evolution; ISM: clouds; ISM: structure; submillimeter: ISM ID LARGE-MAGELLANIC-CLOUD; CO-TO-H-2 CONVERSION FACTOR; FINE-STRUCTURE TRANSITION; PHOTON-DOMINATED REGIONS; NEUTRAL ATOMIC PHASES; MILKY-WAY; INTERSTELLAR-MEDIUM; MOLECULAR CLOUDS; 158 MICRON; IRREGULAR GALAXIES AB Context. The [C II] 158 mu m line is an important tool for understanding the life cycle of interstellar matter. Ionized carbon is present in a variety of phases of the interstellar medium (ISM), including the diffuse ionized medium, warm and cold atomic clouds, clouds in transition from atomic to molecular, and dense and warm photon dominated regions. Aims. Velocity-resolved observations of [C II] are the most powerful technique available to disentangle the emission produced by these components. These observations can also be used to trace CO-dark H-2 gas and determine the total mass of the ISM. Methods. The Galactic Observations of Terahertz C+ (GOTC+) project surveys the [C II] 158 mu m line over the entire Galactic disk with velocity-resolved observations using the Herschel/HIFI instrument. We present the first longitude-velocity maps of the [C II] emission for Galactic latitudes b = 0 degrees, +/- 0.5 degrees, and +/- 1.0 degrees. We combine these maps with those of Hi, (CO)-C-12, and (CO)-C-13 to separate the different phases of the ISM and study their properties and distribution in the Galactic plane. Results. [C II] emission is mostly associated with spiral arms, mainly emerging from Galactocentric distances between 4 and 10 kpc. It traces the envelopes of evolved clouds as well as clouds that are in the transition between atomic and molecular. We estimate that most of the observed [C II] emission is produced by dense photon dominated regions (similar to 47%), with smaller contributions from CO-dark H-2 gas (similar to 28%), cold atomic gas (similar to 21%), and ionized gas (similar to 4%). Atomic gas inside the Solar radius is mostly in the form of cold neutral medium (CNM), while the warm neutral medium gas dominates the outer galaxy. The average fraction of CNM relative to total atomic gas is similar to 43%. We find that the warm and diffuse CO-dark H2 is distributed over a larger range of Galactocentric distances (4-11 kpc) than the cold and dense H-2 gas traced by (CO)-C-12 and (CO)-C-13 (4-8 kpc). The fraction of CO-dark H-2 to total H-2 increases with Galactocentric distance, ranging from similar to 20% at 4 kpc to similar to 80% at 10 kpc. On average, CO-dark H-2 accounts for similar to 30% of the molecular mass of the Milky Way. When the CO-dark H-2 component is included, the radial distribution of the CO-to-H-2 conversion factor is steeper than that when only molecular gas traced by CO is considered. Most of the observed [C II] emission emerging from dense photon dominated regions is associated with modest far-ultraviolet fields in the range chi(0) similar or equal to 1-30. C1 [Pineda, J. L.; Langer, W. D.; Velusamy, T.; Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pineda, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Jorge.Pineda@jpl.nasa.gov RI Goldsmith, Paul/H-3159-2016; OI Pineda, Jorge/0000-0001-8898-2800 FU National Aeronautics and Space Administration FX This research was conducted at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. We thank the staffs of the ESA and NASA Herschel Science Centers for their help. We would like to thank Roberto Assef for enlightening discussions. The Galactic Arecibo L-Band Feed Array Hi (GALFA-H I) Survey data set was obtained with the Arecibo L-band Feed Array (ALFA) on the Arecibo 305m telescope. Arecibo Observatory is part of the National Astronomy and Ionosphere Center, formerly operated by Cornell University under Cooperative Agreement with the National Science Foundation of the United States of America. c (C) 2013 California Institute of Technology. Government sponsorship acknowledged. NR 91 TC 48 Z9 48 U1 1 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2013 VL 554 AR A103 DI 10.1051/0004-6361/201321188 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200102 ER PT J AU Chae, CS Johnson, JT AF Chae, Chun-Sik Johnson, Joel T. TI A Study of Sea Surface Range-Resolved Doppler Spectra Using Numerically Simulated Low-Grazing-Angle Backscatter Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Doppler radar; Doppler spectrum; low-grazing-angle radar; rough surface scattering; sea surface scattering ID FORWARD-BACKWARD METHOD; ROUGH SURFACES; OCEAN SURFACE; SCATTERING; ACCELERATION; COMPUTATION; RADAR; SHIFT; BAND AB A numerical study of sea surface range-resolved Doppler spectra using low-grazing-angle backscatter measurements is described. Backscattered fields as a function of frequency are computed using the method of moments (MOM) for a single realization of a 1-D oceanlike surface profile as the realization evolves in time. Transformation into the range-Doppler domain enables examination of properties of the resulting Doppler spectra (for both HH and VV polarizations) and their relationship to properties of the surface profile. In general, a strong correspondence between the "long-wave" orbital velocity of the surface projected along the radar line of sight and the Doppler centroid frequency is observed for visible portions of the surface, as well as some evidence of relationships between the "width" of the Doppler spectrum and variations of the projected velocity in time at a given range point. Evidence of similar relationships even in some shadowed portions of the surface is also provided. Doppler spectra from HH and VV polarizations are qualitatively similar, despite differences in total power levels, although the portion of shadowed surface points from which Doppler information is available is somewhat larger in VV polarization. A further examination is conducted using backscattered fields computed with a single-scattering method, which neglects shadowing and any multiple-scattering effects. The remarkable similarities observed between MOM and single-scattered Doppler spectra even in some shadowed portions of the surface suggest that non-line-of-sight propagation effects do not significantly influence Doppler properties in such regions. C1 [Chae, Chun-Sik; Johnson, Joel T.] Ohio State Univ, Dept Elect & Comp Engn, ElectroSci Lab, Columbus, OH 43212 USA. RP Chae, CS (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM chun.sik.chae@jpl.nasa.gov; johnson@ece.osu.edu NR 25 TC 8 Z9 10 U1 0 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2013 VL 51 IS 6 BP 3452 EP 3460 DI 10.1109/TGRS.2012.2223216 PN 1 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 171PE UT WOS:000320940600021 ER PT J AU Khankhoje, UK van Zyl, JJ Cwik, TA AF Khankhoje, Uday K. van Zyl, Jakob J. Cwik, Thomas A. TI Computation of Radar Scattering From Heterogeneous Rough Soil Using the Finite-Element Method SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Electromagnetic scattering by rough surfaces; finite-element methods (FEMs); Monte Carlo simulations; subsurface sensing ID MONTE-CARLO SIMULATIONS; SURFACE SCATTERING; ELECTROMAGNETIC SCATTERING; NUMERICAL-SIMULATION; BISTATIC SCATTERING; BOUNDARY-CONDITIONS; MOISTURE; WAVE; ABSORPTION; EQUATIONS AB A 2-D vector-element-based finite-element method (FEM) is used to calculate the radar backscatter from 1-D bare rough soil surfaces which can have an underlying heterogeneous substrate. Monte Carlo simulation results are presented for scattering at L-band (lambda = 0.24 m). For homogeneous soils with rough surfaces, the results of FEM are compared with the predictions of the small perturbation method. In the case of heterogeneous substrates, soil moisture (and, hence, soil permittivity) is assumed to vary as a function of depth. In this case, the results of FEM are compared with those of the transfer matrix method for flat soil surfaces. In both cases, a good agreement is found. For homogeneous rough soils, it is found that polarimetric radar backscatter and copolarized phase difference have a nonlinear relationship with soil moisture. Finally, it is found that the nature of the soil moisture variation in the top few centimeters of the soil has a strong influence on the backscatter and, hence, on the inferred soil moisture content. C1 [Khankhoje, Uday K.; van Zyl, Jakob J.; Cwik, Thomas A.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Khankhoje, UK (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA. EM uday@alumni.caltech.edu; jakob.j.vanzyl@jpl.nasa.gov; thomas.a.cwik@jpl.nasa.gov OI Khankhoje, Uday/0000-0002-9629-3922 NR 36 TC 8 Z9 8 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2013 VL 51 IS 6 BP 3461 EP 3469 DI 10.1109/TGRS.2012.2225431 PN 1 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 171PE UT WOS:000320940600022 ER PT J AU Che, H Drake, JF Swisdak, M Goldstein, ML AF Che, H. Drake, J. F. Swisdak, M. Goldstein, M. L. TI The adiabatic phase mixing and heating of electrons in Buneman turbulence SO PHYSICS OF PLASMAS LA English DT Article ID MAGNETIC RECONNECTION; PLASMA TURBULENCE; INSTABILITY; MECHANISM; EVOLUTION AB The nonlinear development of the strong Buneman instability and the associated fast electron heating in thin current layers with Omega(e)/omega(pe) < 1 is explored. Phase mixing of the electrons in wave potential troughs and a rapid increase in temperature are observed during the saturation of the instability. We show that the motion of trapped electrons can be described using a Hamiltonian formalism in the adiabatic approximation. The process of separatrix crossing as electrons are trapped and de-trapped is irreversible and guarantees that the resulting electron energy gain is a true heating process. (C) 2013 AIP Publishing LLC. C1 [Che, H.; Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Drake, J. F.; Swisdak, M.] Univ Maryland, IREAP, College Pk, MD 20742 USA. RP Che, H (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU NASA Postdoctoral Program at NASA/GSFC; NASA FX This research was supported by the NASA Postdoctoral Program at NASA/GSFC administered by Oak Ridge Associated Universities through a contract with NASA. The simulations and analysis were partially carried out at NASA/Ames High-End Computing Capacity, at the National Energy Research Scientific Computing Center and at the National Institute for Computation Sciences, on Kraken. NR 26 TC 9 Z9 9 U1 0 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 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD JUN PY 2013 VL 20 IS 6 AR 061205 DI 10.1063/1.4811137 PG 4 WC Physics, Fluids & Plasmas SC Physics GA 175ZT UT WOS:000321273200007 ER PT J AU Hesse, M Aunai, N Zenitani, S Kuznetsova, M Birn, J AF Hesse, Michael Aunai, Nicolas Zenitani, Seiji Kuznetsova, Masha Birn, Joachim TI Aspects of collisionless magnetic reconnection in asymmetric systems SO PHYSICS OF PLASMAS LA English DT Article ID FIELD; MAGNETOPAUSE AB Asymmetric reconnection is being investigated by means of particle-in-cell simulations. The research has two foci: the direction of the reconnection line in configurations with nonvanishing magnetic fields; and the question why reconnection can be faster if a guide field is added to an otherwise unchanged asymmetric configuration. We find that reconnection prefers a direction, which maximizes the available magnetic energy, and show that this direction coincides with the bisection of the angle between the asymptotic magnetic fields. Regarding the difference in reconnection rates between planar and guide field models, we demonstrate that a guide field can provide essential confinement for particles in the reconnection region, which the weaker magnetic field in one of the inflow directions cannot necessarily provide. (C) 2013 AIP Publishing LLC. C1 [Hesse, Michael; Aunai, Nicolas; Kuznetsova, Masha] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Zenitani, Seiji] Natl Astron Observ Japan, Tokyo, Japan. [Birn, Joachim] Space Sci Inst, Boulder, CO 80301 USA. RP Hesse, M (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Code 670, Greenbelt, MD 20771 USA. RI Zenitani, Seiji/D-7988-2013; feggans, john/F-5370-2012; NASA MMS, Science Team/J-5393-2013 OI Zenitani, Seiji/0000-0002-0945-1815; NASA MMS, Science Team/0000-0002-9504-5214 FU NASA; NASA's NPP program FX The authors gratefully acknowledge support by NASA's MMS mission and SR&T program. One of us (NA) gratefully acknowledges support from NASA's NPP program. NR 17 TC 18 Z9 18 U1 2 U2 10 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 JUN PY 2013 VL 20 IS 6 AR 061210 DI 10.1063/1.4811467 PG 7 WC Physics, Fluids & Plasmas SC Physics GA 175ZT UT WOS:000321273200012 ER PT J AU Pullen, AR Hirata, CM AF Pullen, Anthony R. Hirata, Christopher M. TI Systematic Effects in Large-Scale Angular Power Spectra of Photometric Quasars and Implications for Constraining Primordial Non-Gaussianity SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; INFLATIONARY UNIVERSE SCENARIO; GALAXY SURVEYS; DATA RELEASE; SDSS-III; PERTURBATIONS; SAMPLE; FLUCTUATIONS; GENERATION AB Primordial non-Gaussianity of local type is predicted to lead to enhanced halo clustering on very large scales. Photometric quasars, which can be seen from cosmological redshifts z > 2 even in wide-shallow optical surveys, are promising tracers for constraining non-Gaussianity using this effect. However, large-scale systematics can also mimic this signature of non-Gaussianity. In order to assess the contribution of systematic effects, we cross-correlate overdensity maps of photometric quasars from the Sloan Digital Sky Survey (SDSS) Data Release 6 (DR6) in different redshift ranges. We find that the maps are significantly correlated on large scales, even though we expect the angular distributions of quasars at different redshifts to be uncorrelated. This implies that the quasar maps are contaminated with systematic errors. We investigate the use of external templates that provide information on the spatial dependence of potential systematic errors to reduce the level of spurious clustering in the quasar data. We find that templates associated with stellar density, the stellar color locus, airmass, and seeing are major contaminants of the quasar maps, with seeing having the largest effect. Using template projection, we are able to decrease the significance of the cross-correlation measurement on the largest scales from 9.2 sigma to 5.4 sigma. Although this is an improvement, the remaining cross-correlation suggests the contamination in this quasar sample is too great to allow a competitive constraint on f(NL) by correlations internal to this sample. The SDSS quasar catalog exhibits spurious number density fluctuations of approximately 2% rms, and we need a contamination level less than 1% (0.6%) in order to measure values of f(NL) less than 100 (10). Properly dealing with be paramount for future large scale structure surveys that seek to constrain non-Gaussianity. C1 [Pullen, Anthony R.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. [Hirata, Christopher M.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. RP Pullen, AR (reprint author), CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr,MS 169-234, Pasadena, CA 91109 USA. EM anthony.r.pullen@jpl.nasa.gov RI Pullen, Anthony/I-7007-2015 OI Pullen, Anthony/0000-0002-2091-8738 NR 71 TC 23 Z9 24 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2013 VL 125 IS 928 BP 705 EP 718 DI 10.1086/671189 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 172JX UT WOS:000321000400009 ER PT J AU Nakata, M Sano, I Mukai, S Holben, BN AF Nakata, Makiko Sano, Itaru Mukai, Sonoyo Holben, Brent N. TI Spatial and Temporal Variations of Atmospheric Aerosol in Osaka SO ATMOSPHERE LA English DT Article DE atmospheric particles; dust storm; radiation simulation; ground measurements; SEM/EDX ID SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; ACE-ASIA; AERONET; NETWORK; MODEL; DUST; TRANSPORT; QUALITY; SUN AB It is well known that the aerosol distribution in Asia is complex due to both the increasing emissions of the anthropogenic aerosols associated with economic growth and the behavior of natural dusts. Therefore, detailed observations of atmospheric particles in Asian urban cities are important. In this work, we focus on the spatial and temporal variations of atmospheric particles around Higashi-Osaka in Japan. Higashi-Osaka is located in the eastern part of Osaka, the second-largest city in Japan, and is famous for small-and medium-sized manufacturing enterprises. For this study, we placed various ground measurement devices around the Higashi-Osaka campus of Kinki University including a Cimel sunphotometer supported by NASA/AERONET (Aerosol robotics network), suspended particulate matter (SPM) sampler and LIDAR (light detection and ranging). Individual particle analyses with a SEM (scanning electron microscope)/EDX (energy-dispersive X-ray analyzer) show the temporal variations of particle properties, such as size, shape and components, during a dust event on 21 March 2010. The simultaneous measurement using a portable sun photometer with AERONET was conducted from April to November 2011. A comparison of the data at each site and the combination of the observed LIDAR data and model simulations indicate the difference in the transportation processes between dust and anthropogenic particles. We suppose this difference is attributed to the differences in the vertical aerosol profiles, where one aerosol is transported over Mount Ikoma and the other is blocked by it. C1 [Nakata, Makiko] Kinki Univ, Fac Appl Sociol, Higashi Osaka 5778502, Japan. [Sano, Itaru; Mukai, Sonoyo] Kinki Univ, Grad Sch Sci & Technol, Higashi Osaka 5778502, Japan. [Holben, Brent N.] NASA, GSFC, Greenbelt, MD 20771 USA. RP Nakata, M (reprint author), Kinki Univ, Fac Appl Sociol, 3-4-1 Kowakae, Higashi Osaka 5778502, Japan. EM nakata@socio.kindai.ac.jp; sano@info.kindai.ac.jp; mukai@info.kindai.ac.jp; brent.n.holben@nasa.gov FU Japan Society for the Promotion of Science [23120708]; Global Change Observation Mission-Climate (GCOM-C) by JAXA [JX-PSPC-308878] FX The authors thank NASA/AERONET team for data processing. This work was supported in part by a Grant-in-Aid for Scientific Research from the Japan Society for the Promotion of Science (No. 23120708) and by Global Change Observation Mission-Climate (GCOM-C) by JAXA (No. JX-PSPC-308878). NR 25 TC 5 Z9 5 U1 1 U2 12 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2073-4433 J9 ATMOSPHERE-BASEL JI Atmosphere PD JUN PY 2013 VL 4 IS 2 BP 157 EP 168 DI 10.3390/atmos4020157 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 175RZ UT WOS:000321251200005 ER PT J AU Pozzi, W Sheffield, J Stefanski, R Cripe, D Pulwarty, R Vogt, JV Heim, RR Brewer, MJ Svoboda, M Westerhoff, R van Dijk, AIJM Lloyd-Hughes, B Pappppenberger, F Werner, M Dutra, E Wetterhall, F Wagner, W Schubert, S Mo, KT Nicholson, M Bettio, L Nunez, L van Beek, R Bierkens, M de Goncalves, LGG De Mattos, JGZ Lawford, R AF Pozzi, Will Sheffield, Justin Stefanski, Robert Cripe, Douglas Pulwarty, Roger Vogt, Juergen V. Heim, Richard R., Jr. Brewer, Michael J. Svoboda, Mark Westerhoff, Rogier van Dijk, Albert I. J. M. Lloyd-Hughes, Benjamin Pappppenberger, Florian Werner, Micha Dutra, Emanuel Wetterhall, Fredrik Wagner, Wolfgang Schubert, Siegfried Mo, Kingtse Nicholson, Margaret Bettio, Lynette Nunez, Liliana van Beek, Rens Bierkens, Marc Goncalves de Goncalves, Luis Gustavo Zell de Mattos, Joao Gerd Lawford, Richard TI TOWARD GLOBAL DROUGHT EARLY WARNING CAPABILITY: Expanding International Cooperation for the Development of a Framework for Monitoring and Forecasting SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID SUB-SAHARAN AFRICA; SOIL-MOISTURE; UNITED-STATES; 20TH-CENTURY DROUGHT; FOOD SECURITY AB Drought is a global problem that has far-reaching impacts, especially on vulnerable populations in developing regions. This paper highlights the need for a Global Drought Early Warning System (GDEWS), the elements that constitute its underlying framework (GDEWF), and the recent progress made toward its development. Many countries lack drought monitoring systems, as well as the capacity to respond via appropriate political, institutional, and technological frameworks, and these have inhibited the development of integrated drought management plans or early warning systems. The GDEWS will provide a source of drought tools and products via the GDEWF for countries and regions to develop tailored drought early warning systems for their own users. A key goal of a GDEWS is to maximize the lead time for early warning, allowing drought managers and disaster coordinators more time to put mitigation measures in place to reduce the vulnerability to drought. To address this, the GDEWF will take both a top-down approach to provide global realtime drought monitoring and seasonal forecasting, and a bottom-up approach that builds upon existing national and regional systems to provide continental-to-global coverage. A number of challenges must be overcome, however, before a GDEWS can become a reality, including the lack of in situ measurement networks and modest seasonal forecast skill in many regions, and the lack of infrastructure to translate data into useable information. A set of international partners, through a series of recent workshops and evolving collaborations, has made progress toward meeting these challenges and developing a global system. C1 [Pozzi, Will; Wagner, Wolfgang] Vienna Univ Technol, Inst Photogrammetry & Remote Sensing IPF, A-1040 Vienna, Austria. [Sheffield, Justin] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Stefanski, Robert] World Meteorol Org, Climate & Water Dept, Agr Meteorol Div, Geneva, Switzerland. [Cripe, Douglas] Grp Earth Observ Secretariat, Geneva, Switzerland. [Pulwarty, Roger] Natl Integrated Drought Informat Syst, Boulder, CO USA. [Vogt, Juergen V.] Commiss European Communities, Joint Res Ctr, I-21020 Ispra, Italy. [Heim, Richard R., Jr.; Brewer, Michael J.] NOAA, Natl Climat Data Ctr, Asheville, NC USA. [Westerhoff, Rogier; Werner, Micha] Deltares, Delft, Netherlands. [van Dijk, Albert I. J. M.] CSIRO, Canberra, ACT, Australia. [van Dijk, Albert I. J. M.] Australian Natl Univ, Canberra, ACT, Australia. [Pappppenberger, Florian; Dutra, Emanuel; Wetterhall, Fredrik] European Ctr Medium Range Weather Forecasts, Predictabil & Diagnost Sect, Reading RG2 9AX, Berks, England. [Werner, Micha] UNESCO IHE, Delft, Netherlands. [Lloyd-Hughes, Benjamin] Univ Reading, Walker Inst, Reading RG6 2AH, Berks, England. [Svoboda, Mark] Natl Drought Mitigat Ctr, Monitoring Program Area, Lincoln, NE USA. [Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mo, Kingtse] NOAA, US Ctr Climate Predict, Washington, DC USA. [Nicholson, Margaret] Australia Bur Agr & Econ Sci, Canberra, ACT, Australia. [Nunez, Liliana] Argentina Serv Meteorol Nacl, Buenos Aires, DF, Argentina. [Bettio, Lynette] Bur Meteorol, Natl Climate Ctr, Melbourne, Vic, Australia. [van Beek, Rens; Bierkens, Marc] Univ Utrecht, NL-3508 TC Utrecht, Netherlands. [Goncalves de Goncalves, Luis Gustavo; Zell de Mattos, Joao Gerd] Inst Nacl Pesquisas Espaciais, Ctr Previsao Tempo & Estudos Climat, Sao Paulo, Brazil. [Lawford, Richard] Morgan State Univ, Baltimore, MD 21239 USA. RP Pozzi, W (reprint author), Vienna Univ Technol, Inst Photogrammetry & Remote Sensing IPF, Gusshausstr 27-29, A-1040 Vienna, Austria. EM will.pozzi@gmail.com RI Werner, Micha/C-8144-2009; Wetterhall, Fredrik/I-2374-2012; Pappenberger, Florian/A-2839-2009; Dutra, Emanuel/A-3774-2010; Van Dijk, Albert/B-3106-2011; van Beek, Rens/B-4904-2014; OI Werner, Micha/0000-0003-4198-5638; Wetterhall, Fredrik/0000-0001-5331-9064; Pappenberger, Florian/0000-0003-1766-2898; Dutra, Emanuel/0000-0002-0643-2643; Van Dijk, Albert/0000-0002-6508-7480; van Beek, Rens/0000-0002-4758-108X; Wagner, Wolfgang/0000-0001-7704-6857 NR 26 TC 38 Z9 38 U1 5 U2 51 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD JUN PY 2013 VL 94 IS 6 BP 776 EP 785 DI 10.1175/BAMS-D-11-00176.1 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 175TK UT WOS:000321256100001 ER PT J AU Peterson, TC Heim, RR Hirsch, R Kaiser, DP Brooks, H Diffenbaugh, NS Dole, RM Giovannettone, JP Guirguis, K Karl, TR Katz, RW Kunkel, K Lettenmaier, D McCabe, GJ Paciorek, CJ Ryberg, KR Schubert, S Silva, VBS Stewart, BC Vecchia, AV Villarini, G Vose, RS Walsh, J Wehner, M Wolock, D Wolter, K Woodhouse, CA Wuebbles, D AF Peterson, Thomas C. Heim, Richard R., Jr. Hirsch, Robert Kaiser, Dale P. Brooks, Harold Diffenbaugh, Noah S. Dole, Randall M. Giovannettone, Jason P. Guirguis, Kristen Karl, Thomas R. Katz, Richard W. Kunkel, Kenneth Lettenmaier, Dennis McCabe, Gregory J. Paciorek, Christopher J. Ryberg, Karen R. Schubert, Siegfried Silva, Viviane B. S. Stewart, Brooke C. Vecchia, Aldo V. Villarini, Gabriele Vose, Russell S. Walsh, John Wehner, Michael Wolock, David Wolter, Klaus Woodhouse, Connie A. Wuebbles, Donald TI MONITORING AND UNDERSTANDING CHANGES IN HEAT WAVES, COLD WAVES, FLOODS, AND DROUGHTS IN THE UNITED STATES: State of Knowledge SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID SOUTHWESTERN NORTH-AMERICA; SOIL-MOISTURE; CLIMATE-CHANGE; WATER MANAGEMENT; GREAT-PLAINS; NEW-ENGLAND; DUST-BOWL; US; TEMPERATURE; STREAMFLOW AB Weather and climate extremes have been varying and changing on many different time scales. In recent decades, heat waves have generally become more frequent across the United States, while cold waves have been decreasing. While this is in keeping with expectations in a warming climate, it turns out that decadal variations in the number of U.S. heat and cold waves do not correlate well with the observed U.S. warming during the last century. Annual peak flow data reveal that river flooding trends on the century scale do not show uniform changes across the country. While flood magnitudes in the Southwest have been decreasing, flood magnitudes in the Northeast and north-central United States have been increasing. Confounding the analysis of trends in river flooding is multiyear and even multidecadal variability likely caused by both large-scale atmospheric circulation changes and basin-scale memory in the form of soil moisture. Droughts also have long-term trends as well as multiyear and decadal variability. Instrumental data indicate that the Dust Bowl of the 1930s and the drought in the 1950s were the most significant twentieth-century droughts in the United States, while tree ring data indicate that the megadroughts over the twelfth century exceeded anything in the twentieth century in both spatial extent and duration. The state of knowledge of the factors that cause heat waves, cold waves, floods, and drought to change is fairly good with heat waves being the best understood. C1 [Peterson, Thomas C.; Heim, Richard R., Jr.; Vose, Russell S.] NOAA, Natl Climat Data Ctr, Asheville, NC 28803 USA. [Hirsch, Robert] US Geol Survey, Reston, VA 22092 USA. [Kaiser, Dale P.] US DOE, Carbon Dioxide Informat Anal Ctr, Oak Ridge Natl Lab, Oak Ridge, TN USA. [Brooks, Harold] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Diffenbaugh, Noah S.] Stanford Univ, Stanford, CA 94305 USA. [Dole, Randall M.; Wolter, Klaus] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Giovannettone, Jason P.] US Army Corp Engineers, Inst Water Resources, Alexandria, VA USA. [Guirguis, Kristen] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Guirguis, Kristen] Univ Corp Atmospher Res, Boulder, CO USA. [Katz, Richard W.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Kunkel, Kenneth] Cooperat Inst Climate & Satellites, Asheville, NC USA. [Lettenmaier, Dennis] Univ Washington, Seattle, WA 98195 USA. [McCabe, Gregory J.; Wolock, David] USGS, Lawrence, KS USA. [Paciorek, Christopher J.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [Ryberg, Karen R.; Vecchia, Aldo V.] US Geol Survey, Bismarck, ND USA. [Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Silva, Viviane B. S.] NOAA, Climate Serv Div, NWS, OCWWS, Silver Spring, MD USA. [Stewart, Brooke C.] STG, Asheville, NC USA. [Villarini, Gabriele] Univ Iowa, IIHR Hydrosci & Engn, Iowa City, IA USA. [Walsh, John] Univ Alaska Fairbanks, Fairbanks, AK USA. [Wehner, Michael] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Woodhouse, Connie A.] Univ Arizona, Tucson, AZ USA. [Wuebbles, Donald] Univ Illinois, Urbana, IL USA. RP Peterson, TC (reprint author), NOAA, Natl Climat Data Ctr, 151 Patton Ave, Asheville, NC 28803 USA. EM thomas.c.peterson@noaa.gov RI lettenmaier, dennis/F-8780-2011; Diffenbaugh, Noah/I-5920-2014; Kunkel, Kenneth/C-7280-2015; Wolter, Klaus/D-5988-2015; Katz, Richard/K-4133-2012; Ryberg, Karen/E-1871-2016; Villarini, Gabriele/F-8069-2016; OI lettenmaier, dennis/0000-0003-3317-1327; Diffenbaugh, Noah/0000-0002-8856-4964; Kunkel, Kenneth/0000-0001-6667-7047; Katz, Richard/0000-0002-0267-8953; Ryberg, Karen/0000-0002-9834-2046; Villarini, Gabriele/0000-0001-9566-2370; Hirsch, Robert/0000-0002-4534-075X NR 95 TC 84 Z9 85 U1 10 U2 132 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD JUN PY 2013 VL 94 IS 6 BP 821 EP 834 DI 10.1175/BAMS-D-12-00066.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 175TK UT WOS:000321256100005 ER PT J AU Roegner, GC Daly, EA Brodeur, RD AF Roegner, G. Curtis Daly, Elizabeth A. Brodeur, Richard D. TI Surface distribution of brachyuran megalopae and ichthyoplankton in the Columbia River plume during transition from downwelling to upwelling conditions SO CONTINENTAL SHELF RESEARCH LA English DT Article DE Columbia River plume; Crab megalopae; Juvenile fishes; Neuston; Upwelling; California Current ID CRAB CANCER-MAGISTER; NORTHERN CALIFORNIA CURRENT; DUNGENESS CRAB; OCEANOGRAPHIC CONDITIONS; COMMUNITY STRUCTURE; RECRUITMENT LIMITATION; SPATIAL-DISTRIBUTION; JUVENILE SALMONIDS; VERTICAL MIGRATION; WILLAPA BAY AB In the California Current coastal boundary zone, the spring transition between downwelling and upwelling conditions, along with the fluctuating structure of the Columbia River plume, creates highly dynamic interactions. In this study, we investigated whether the surface distribution of brachyuran larvae and ichthyoplankton would track the dynamics of the Columbia River plume. By happenstance, the cruise period coincided with the spring transition from downwelling to sustained upwelling conditions in 2010, a year when the transition was delayed and Columbia River flow was substantially higher than average. We used time series of wind and freshwater input to evaluate the influence of physical forcing on oceanographic patterns, and sampled hydrography and surface plankton concentrations within a 182 km(2) grid off Willapa Bay, WA. Additionally, two longer transects, one cross-shelf and the other along-shore, were made to discern the extent of plume influence on larval crab and fish abundance. We found that plume waters that were trapped in a northward-flowing coastal-boundary current during downwelling conditions were advected offshore after several days of upwelling-favorable winds. Neustonic collections of brachyuran larvae and ichthyoplankton varied in response to this large seaward advective event. Megalopae of cancrid crabs exhibited patterns of both offshore transport (Cancer oregonensis/productus) and nearshore retention (C. magister). Additionally, abundant numbers of large juvenile widow (Sebastes entomelas) and yellowtail (S. flavidus) rockfish of a size appropriate for settlement were sampled during a period when ocean conditions favored high recruitment success. These results demonstrated that the response of planktonic crab larvae and ichthyoplankton to large-scale advection varied by species, with larger and more vagile fish exhibiting less evidence of passive transport than smaller crab larvae. Importantly, portions of the planktonic fish and crab community were able to maintain nearshore distributions in favorable settlement habitat, despite physical advection offshore. Published by Elsevier Ltd. C1 [Roegner, G. Curtis] NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Point Adams Res Stn, Hammond, OR 97121 USA. [Daly, Elizabeth A.] Oregon State Univ, Cooperat Inst Marine Resources Studies, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. [Brodeur, Richard D.] NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Roegner, GC (reprint author), NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Point Adams Res Stn, POB 155, Hammond, OR 97121 USA. EM Curtis.Roegner@noaa.gov FU Bonneville Power Administration; National Marine Fisheries Service FX We sincerely thank scientists Sarikka Attoe, Caren Barcelo, and Amanda Gladics, and electronic technicians Manuel Calderon and Phil White for help with the sampling. Toby Auth, JoAnne Butzerin, Jennifer Fisher, and Kurt Fresh provided very helpful comments on an earlier version of the manuscript. Funding for this research was provided by Bonneville Power Administration and the National Marine Fisheries Service. NR 60 TC 5 Z9 5 U1 2 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 J9 CONT SHELF RES JI Cont. Shelf Res. PD JUN 1 PY 2013 VL 60 BP 70 EP 86 DI 10.1016/j.csr.2013.04.007 PG 17 WC Oceanography SC Oceanography GA 174QW UT WOS:000321171500007 ER PT J AU Chan, KL Mayr, HG AF Chan, Kwing L. Mayr, Hans G. TI Numerical simulation of convectively generated vortices: Application to the Jovian planets SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE vortices; convection; giant planets; Great Red Spot; White Ovals ID GREAT-RED-SPOT; SHALLOW-WATER TURBULENCE; NONLINEAR SIMULATIONS; ROTATING CONVECTION; VERTICAL STRUCTURE; GIANT PLANETS; COMPRESSIBLE CONVECTION; JUPITER; JETS; MODEL AB Numerical experiments are performed to study the possibility of long-lived vortex generation in rotating convection zones. The domain of computation is a rectangular box with fixed latitude. The fully compressible fluid equations are solved using an explicit, strongly conservative finite difference method. A total of eight cases covering two different latitudes and four different rotation rates were computed. As the rotation rate increases, a long-lived cyclone first appears. The high latitude environment is more favorable for vortex formation. An anticyclone appears when the rotation is adequately fast. Possible implications of the numerical results to the Jovian planets are discussed. (C) 2013 Elsevier B.V. All rights reserved. C1 [Chan, Kwing L.] Hong Kong Univ Sci & Technol, Dept Math, Hong Kong, Hong Kong, Peoples R China. [Mayr, Hans G.] Hong Kong Univ Sci & Technol, Ctr Space Sci Res, Hong Kong, Hong Kong, Peoples R China. [Mayr, Hans G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mayr, Hans G.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Chan, KL (reprint author), Hong Kong Univ Sci & Technol, Dept Math, Hong Kong, Hong Kong, Peoples R China. EM maklchan@ust.hk OI Chan, Kwing/0000-0002-6428-1812 FU Hong Kong Research Grants Council [HKUST 600309] FX We thank the anonymous reviewers for comments leading to improvement of the manuscript KLC thanks the Hong Kong Research Grants Council for support (HKUST 600309). NR 44 TC 6 Z9 6 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JUN PY 2013 VL 371 BP 212 EP 219 DI 10.1016/j.epsl.2013.03.046 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 173KC UT WOS:000321077400021 ER PT J AU Reeves, JD Eveleigh, T Holzer, TH Sarkani, S AF Reeves, John D. Eveleigh, Tim Holzer, Thomas H. Sarkani, Shahryar TI Risk Identification Biases and Their Impact to Space System Development Project Performance SO EMJ-ENGINEERING MANAGEMENT JOURNAL LA English DT Article DE Engineering Management; Program and Project Management; Risk Management; Systems Engineering AB Risk identification during the design and development phases of complex systems is commonly implemented, but often fails to result in the identification of events and circumstances that truly challenge project performance. Inefficiencies in cost and schedule estimation are usually held accountable for cost and schedule overruns, but the true root cause is often the realization of programmatic and technical risks. This research explores risk identification trends and biases pervasive during space system development that limit the awareness of such risks. The findings and results provide insight into how future engineering and risk managers can potentially avoid these shortfalls. C1 [Reeves, John D.] NASA, Langley Res Ctr, Space Mission Anal Branch, Hampton, VA 23681 USA. [Eveleigh, Tim; Holzer, Thomas H.] George Washington Univ, Washington, DC 20052 USA. [Sarkani, Shahryar] George Washington Univ, Dept Engn Management & Syst Engn, Washington, DC 20052 USA. RP Reeves, JD (reprint author), NASA, Langley Res Ctr, MS 426, Hampton, VA 23681 USA. EM john.d.reeves@nasa.gov NR 17 TC 2 Z9 2 U1 0 U2 9 PU AMER SOC ENGINEERING MANAGEMENT PI ROLLA PA PO BOX 820, ROLLA, MO 65402 USA SN 1042-9247 J9 EMJ-ENG MANAG J JI EMJ-Eng. Manag. J. PD JUN PY 2013 VL 25 IS 2 SI SI BP 3 EP 12 PG 10 WC Engineering, Industrial; Management SC Engineering; Business & Economics GA 174MA UT WOS:000321158400003 ER PT J AU Zhou, DK Larar, AM Liu, X AF Zhou, Daniel K. Larar, Allen M. Liu, Xu TI MetOp-A/IASI Observed Continental Thermal IR Emissivity Variations SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Geophysical inverse problems; infrared measurements; remote sensing; satellite applications; surface emissivity ID LAND-SURFACE EMISSIVITY AB Satellite thermal infrared (IR) spectral emissivity data have been shown to be significant for atmospheric research and monitoring the Earth's environment. Long-term and large-scale observations that are needed for global monitoring and research can only be supplied by satellite-based remote sensing. Presented here is the global surface IR emissivity data retrieved from the last five and half years of Infrared Atmospheric Sounding Interferometer (IASI) measurements observed from the MetOp-A satellite. Monthly mean surface properties (i.e., skin temperature T-s and spectral emissivity epsilon(nu)) with a spatial resolution of 0.5 x 0.5-degrees latitude-longitude are produced to monitor seasonal and inter-annual variations. Continental IR spectral emissivity derived from satellite ultraspectral IR measurements reveals its variation depending on surface weather and climate conditions. Variation behaviors of continental IR spectral emissivity, associated with the seasonal change as well as weather and climate conditions are initially captured by IASI measurements and will be continuously monitored as provided by the satellite measurements. Surface epsilon(nu) retrieved with IASI measurements can be used to assist in monitoring surface weather and surface climate change. Surface epsilon(nu) together with T-s from current and future operational weather satellites can be utilized as a means of long-term and large-scale monitoring of Earth's surface weather environment and associated changes. C1 [Zhou, Daniel K.; Larar, Allen M.; Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23693 USA. RP Zhou, DK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23693 USA. EM daniel.k.zhou@nasa.gov RI Richards, Amber/K-8203-2015 FU NASA Langley Research Center; NASA Headquarters FX IASI was developed and built under the responsibility of the Centre National d'Etudes Spatiales (CNES). It is flown aboard the MetOp satellites as part of the EUMETSAT Polar System. The IASI L1C data are received through NOAA Comprehensive Large Array-data Stewardship System (CLASS). This research is supported by NASA Langley Research Center and NASA Headquarters. The authors are grateful to Dr. L. Larrabee Strow (University of Maryland-Baltimore County) and Dr. Ping Yang (Texas A&M University) for providing the fast molecular and cloud radiative transfer models, and also grateful to Prof. William L. Smith, Sr. (University of Wisconsin-Madison and Hampton University) for his encouragement. The authors wish to acknowledge support from NASA Headquarters Research Division Director Dr. Jack Kaye, and to extend their appreciation to the anonymous reviewers. NR 22 TC 1 Z9 1 U1 2 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1156 EP 1162 DI 10.1109/JSTARS.2013.2238892 PG 7 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800012 ER PT J AU Parkinson, CL AF Parkinson, Claire L. TI Summarizing the First Ten Years of NASA's Aqua Mission SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Satellite Earth observations; Aqua; global energy budget; water cycle ID AMSR-E; MODIS; CLIMATE; SYSTEM; WATER; TEMPERATURE; RETRIEVALS; VALIDATION; SCIENCE; IMPACT AB The Aqua spacecraft was launched on May 4, 2002 with six Earth-observing instruments on board to collect data on a wide variety of Earth system variables. After ten years of on-orbit operations, Aqua has provided data that have contributed to over 2 000 scientific publications, with new results on the Earth's energy budget, trace gases and particulate matter in the atmosphere, vegetation on land and in the oceans, and many aspects of the water cycle, including evaporation and transpiration, water vapor, cloud cover, precipitation, the oceans, sea ice and land ice, snow cover, and soil moisture. Additionally, Aqua data have been used to assist in practical applications ranging from weather forecasting to the deployment of firefighters and the routing of aircraft. Although the six-year design life of the satellite has been successfully completed and exceeded, enough fuel remains on Aqua for approximately another ten years of operations. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Parkinson, CL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM claire.l.parkinson@nasa.gov RI Parkinson, Claire/E-1747-2012 OI Parkinson, Claire/0000-0001-6730-4197 FU Earth Science Division at NASA Headquarters FX This work was funded by the Earth Science Division at NASA Headquarters. NR 50 TC 8 Z9 8 U1 2 U2 29 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1179 EP 1188 DI 10.1109/JSTARS.2013.2239608 PG 10 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800015 ER PT J AU Ramachandran, R Rushing, J Lin, A Conover, H Li, X Graves, S Nair, US Kuo, KS Smith, DK AF Ramachandran, Rahul Rushing, John Lin, Amy Conover, Helen Li, Xiang Graves, Sara Nair, U. S. Kuo, Kwo-Sen Smith, Deborah K. TI Data Prospecting-A Step Towards Data Intensive Science SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Architecture; data analysis; data preprocessing; data systems; data visualization; information retrieval; remote sensing; sea surface ID MONTANE CLOUD FORESTS; ARABIAN SEA; SOMALI-JET; VISUALIZATION; IMPACT AB Data-intensive science is a scientific discovery process that is driven by knowledge extracted from large volumes of data rather than the traditional hypothesis driven discovery process. One of the key challenges in data-intensive science is development of enabling technologies to allow researchers to effectively utilize these large volumes of data in an effective manner. This paper introduces the concept of "data prospecting" to address the challenges of data intensive science. With data prospecting, we extend the familiar metaphor of data mining to describe an initial phase of data exploration used to determine promising areas for deeper analysis. Data prospecting enhances data selection through the use of interactive discovery engines. Interactive exploration enables a researcher to filter the data based on the "first look" analytics, discover interesting and previously unknown patterns to start new science investigations, verify the quality of the data, and corroborate whether patterns in the data match existing science theories or mental models. This paper describes our initial evaluation of the value of"data prospecting" to Earth Science researchers as part of their research process. The paper describes our discovery engine prototype to support data prospecting for specific data products along with its current limitations. Example science investigations from three different researchers using our prototype discovery engine to explore the Special Sensor Microwave/Imager and Sounder (SSM/I, SSMIS) data products are also presented. C1 [Ramachandran, Rahul; Rushing, John; Lin, Amy; Conover, Helen; Li, Xiang; Graves, Sara; Nair, U. S.] Univ Alabama, Huntsville, AL 35899 USA. [Kuo, Kwo-Sen] NASA, Caelum Res Corp, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, Deborah K.] Remote Sensing Syst, Santa Rosa, CA 95401 USA. RP Ramachandran, R (reprint author), Univ Alabama, Huntsville, AL 35899 USA. EM rramachandran@itsc.uah.edu; jrushing@itsc.uah.edu; alin@itsc.uah.edu; hconover@itsc.uah.edu; xli@itsc.uah.edu; sgraves@itsc.uah.edu; nair@nsstc.uah.edu; kwo-sen.kuo@nasa.gov; smith@remss.com OI Ramachandran, Rahul/0000-0002-0647-1941 NR 28 TC 0 Z9 0 U1 0 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1233 EP 1241 DI 10.1109/JSTARS.2013.2248133 PG 9 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800021 ER PT J AU Percivall, GS Alameh, NS Caumont, H Moe, KL Evans, JD AF Percivall, George S., III Alameh, Nadine S. Caumont, Herve Moe, Karen L. Evans, John D. TI Improving Disaster Management Using Earth Observations-GEOSS and CEOS Activities SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Architecture; Committee on Earth Observation Satellites (CEOS); disaster management; earth observations; Group on Earth Observations (GEO); Global Earth Observing System of Systems (GEOSS); interoperability; Open Geospatial Consortium (OGC) AB This paper describes how the Group on Earth Observations (GEO) and the Committee on Earth Observation Satellites (CEOS) are individually and collaboratively strengthening worldwide ability for agencies to manage the disasters lifecycle. The Architecture Implementation Pilot (AIP) of GEO has, through an agile development process, deployed and tested advanced information systems for Earth Observations based on interoperability arrangements. In particular, AIP has focused on several disaster management scenarios resulting in an architecture that has improved the ready viability and usability of data for disasters. CEOS is constructing a reference architecture, intended to streamline access to satellite data and services for disaster management and risk assessment. The CEOS approach aims to support disaster management activities with satellite information in a holistic fashion, taking account of their overlaps and interdependencies. Jointly GEO and CEOS are now working to align the approaches for disaster management to describe enterprise components and improve understanding of contributed systems and their roles. The coordination has lead to refinements of the Disaster Management Scenario via further implementation in AIP-5. By collaborating via the CEOS working groups and the Global Earth Observing System of Systems (GEOSS) communities of practice, these efforts are intended to engage the international community focused on disaster management and risk assessment to fully utilize remote sensing resources for societal benefit. C1 [Percivall, George S., III; Alameh, Nadine S.] Open Geospatial Consortium, Crofton, MD 21114 USA. [Caumont, Herve] Terradue, Paris, France. [Moe, Karen L.] NASA, Earth Sci Technol Off, Greenbelt, MD 20771 USA. [Evans, John D.] Global Sci & Technol Inc, Greenbelt, MD 20770 USA. RP Percivall, GS (reprint author), Open Geospatial Consortium, Crofton, MD 21114 USA. EM gpercivall@opengeospatial.org; nalameh@opengeospatial.org; herve.caumont@ter-radue.com; karen.moe@nasa.gov; john.evans@gst.com NR 28 TC 6 Z9 6 U1 1 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1368 EP 1375 DI 10.1109/JSTARS.2013.2253447 PG 8 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800033 ER PT J AU Liao, L Meneghini, R Nowell, HK Liu, GS AF Liao, Liang Meneghini, Robert Nowell, Holly Kreutzer Liu, Guosheng TI Scattering Computations of Snow Aggregates From Simple Geometrical Particle Models SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Radar; radiometer; scattering; snow ID ICE; APPROXIMATION; DISTRIBUTIONS; FREQUENCIES; SNOWFLAKES AB Scattering results from snowflakes generated from aggregates comprised of 6-branch bullet rosette crystals are compared with those obtained from spherical or spheroidal ice-air mixed phase particles. The scattering parameters of the aggregates are computed by the discrete dipole approximation (DDA) numerical approach at frequencies from 10.65 to 183.31 GHz (where the particular frequencies match those of the Global Precipitation Measurement (GPM) Microwave Imager (GMI) and Dual-frequency Precipitation Radar (DPR)). Two mass density models are used to specify the snow density of the simple geometrical particles. In one model, the density is prescribed as a function of the maximum dimension of the aggregates (variable snow density model); in the other the density is independent of particle size (fixed snow density model). Comparisons of the results indicate that the scattering parameters of large complex aggregates differ significantly from those obtained from the equivalent-mass spherical/spheroidal-shaped particles when variable snow density is assumed. In contrast to the variable snow density model, the scattering properties of the aggregates are fairly well reproduced by the fixed snow density model. Although the results from a fixed snow densities between 0.2 and 0.3 g/cm(3) reveal good overall agreement with those from the aggregates, the value of 0.2 g/cm(3) yields the best agreement for the frequencies less than or equal to 35.6 GHz while the model results with a density set to 0.3 g/cm(3) show the best match with the aggregates at frequencies higher than 35.6 GHz. Moreover, scattering parameters of the randomly-oriented spheroidal ice-airmixtures tend to agree better with those from the aggregates than do spherical snow particles. It is anticipated that these findings will have direct implication for the development of the GPM algorithms for estimates of precipitation rate. C1 [Liao, Liang] Morgan State Univ, Baltimore, MD 21251 USA. [Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nowell, Holly Kreutzer; Liu, Guosheng] Florida State Univ, Tallahassee, FL 32306 USA. RP Liao, L (reprint author), Morgan State Univ, Baltimore, MD 21251 USA. RI Liu, Guosheng/D-3479-2011; Measurement, Global/C-4698-2015 OI Liu, Guosheng/0000-0001-7899-6125; FU NASA Headquarters under NASA's Precipitation Measurement Mission (PMM) [NNH06ZDA001N-PMM] FX This work was supported by Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement Mission (PMM) Grant NNH06ZDA001N-PMM. NR 27 TC 8 Z9 8 U1 2 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1409 EP 1417 DI 10.1109/JSTARS.2013.2255262 PG 9 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800037 ER PT J AU LeCompte, M Bindschadler, R Hayden, LB Jefferson, M Bridgers, YS Lawrence, R Bevins, J Brownlow, J Evans, R Hawk, K Koch, G AF LeCompte, Malcolm Bindschadler, Robert Hayden, Linda Bailey Jefferson, Michael Bridgers, Ya' Shonti Lawrence, Ryan Bevins, Joyce Brownlow, Jessica Evans, Robyn Hawk, Kirsten Koch, Glenn TI Reduction and Loss of an Ice Shelf in Elizabeth City State University Bay, Antarctica: 1972-2003 SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Antarctica; ENVI; grounding line; ice shelf; Landsat ID PINE ISLAND; WEST ANTARCTICA; GLACIER; PENINSULA; ACCELERATION; EMBAYMENT; LARSEN AB Gradual reduction of a small ice shelf in the Pine Island Bay area is measured using eleven Landsat images spanning 1972 to 2003. Measurements of Ice shelf area indicate that it expanded slightly during the first two decades of observations from approximately 6.19 km(2) measured on December 7, 1972 to a maximum of about 6.82 km(2) observed in 1986. This maximum was followed by a nearly continuous decrease in area and ultimate disappearance of the ice shelf by January 17, 2003. No ice shelf has reappeared since 2003 as observed in subsequent Landsat images. Ten of the eleven Landsat images were co-registered and warped to one of a pair of 2003 geographic reference images before area measurement. Individual study team members made independent measurements of the ice shelf area apparent in each image. The average of these measurements had a standard deviation of 0.14 km(2). The specific cause of this ice shelf disappearance is unknown, but is probably related to increased basalmelting by warmer ocean waters reaching Pine Island Bay. Intrusions of warm "Circumpolar Deep Water" are related to ice shelf and outlet glacier thinning and retreat as reported throughout the Amundsen Sea region. This is the first report of complete ice shelf loss so far south or in the Amundsen Bay region. This small, previously unnamed ice shelf formerly occupied what is now known as the Elizabeth City State University Bay. C1 [LeCompte, Malcolm; Hayden, Linda Bailey; Jefferson, Michael; Bridgers, Ya' Shonti; Lawrence, Ryan; Evans, Robyn; Koch, Glenn] Elizabeth City State Univ, Elizabeth City, NC 27909 USA. [Bindschadler, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brownlow, Jessica] Mississippi Valley State Univ, Itta Bena, MS 38941 USA. [Hawk, Kirsten] Spelman Univ, Atlanta, GA 30314 USA. RP LeCompte, M (reprint author), Elizabeth City State Univ, Elizabeth City, NC 27909 USA. FU NASA [NNX08AE01G]; NASA's Cryospheric Sciences program FX This work was supported by NASA Grant NNX08AE01G and NASA's Cryospheric Sciences program. NR 21 TC 0 Z9 0 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1509 EP 1515 DI 10.1109/JSTARS.2013.2258325 PG 7 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800048 ER PT J AU Pan, CH Kowalewski, M Buss, R Flynn, L Wu, XQ Caponi, M Weng, FZ AF Pan, Chunhui Kowalewski, Matthew Buss, Rich Flynn, L. Wu, Xiangqian Caponi, Maria Weng, Fuzhong TI Performance and Calibration of the Nadir Suomi-NPP Ozone Mapping Profiler Suite From Early-Orbit Images SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Calibration; charge coupled device (CCD); Ozone Mapping Profiler Suite (OMPS); remote sensing ID SOLAR; OMPS; UARS AB The Ozone Mapping Profiler Suite (OMPS) was launched aboard the Suomi National Polar-orbiting Partnership spacecraft on October 28, 2011. A successful thorough Early Orbit Checkout (EOC) enabled the current Intensive Calibration and Validation stage. We present our analyses and results of OMPS Nadir early-orbit sensor performance and calibration. We collected and analyzed data from both nominal and diagnostic activities via orbital measurements of detector dark current, sensor linearity, and solar irradiance. Our results demonstrate that the OMPS Nadir sensors smoothly transitioned from ground to orbit by meeting or exceeding sensor level requirements. The orbital measurements agree with the predicted values determined during the prelaunch calibration and characterization of OMPS. Our results also suggest that the effects of charge coupled device (CCD) lattice damage due to energetic particle hits onto the CCD must be accounted for in the dark current calibration. C1 [Pan, Chunhui] Univ Maryland CICS, College Pk, MD 20740 USA. [Pan, Chunhui; Flynn, L.; Wu, Xiangqian; Weng, Fuzhong] NOAA NESDIS Satellite Applicat & Res, College Pk, MD 20740 USA. [Kowalewski, Matthew] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kowalewski, Matthew] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Buss, Rich] Raytheon Corp, Riverdale, MD 20737 USA. [Caponi, Maria] Aerosp Corp, El Segundo, CA 90245 USA. RP Pan, CH (reprint author), Univ Maryland CICS, College Pk, MD 20740 USA. EM chpan@umd.edu RI Flynn, Lawrence/B-6321-2009; Wu, Xiangqian/F-5634-2010; Weng, Fuzhong/F-5633-2010 OI Flynn, Lawrence/0000-0001-6856-2614; Wu, Xiangqian/0000-0002-7804-5650; Weng, Fuzhong/0000-0003-0150-2179 FU NOAA at the University of Maryland [NA09NES4400006] FX This work was supported by NOAA Grant NA09NES4400006 (Cooperative Institute for Climate and Satellites-CICS) at the University of Maryland. NR 14 TC 9 Z9 9 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1539 EP 1551 DI 10.1109/JSTARS.2013.2259144 PG 13 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800052 ER PT J AU Sun, XL Abshire, JB McGarry, JF Neumann, GA Smith, JC Cavanaugh, JF Harding, DJ Zwally, HJ Smith, DE Zuber, MT AF Sun, Xiaoli Abshire, James B. McGarry, Jan F. Neumann, Gregory A. Smith, James C. Cavanaugh, John F. Harding, David J. Zwally, H. Jay Smith, David E. Zuber, Maria T. TI Space Lidar Developed at the NASA Goddard Space Flight Center-The First 20 Years SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Laser altimeter; lidar ID ORBITER LASER ALTIMETER; LUNAR RECONNAISSANCE ORBITER; OPTICAL-SYSTEM DESIGN; MESSENGER MISSION; MERCURY; MARS; PERFORMANCE; INTEGRATION; EARTH; TRANSMITTER AB During the past 20 years the NASA Goddard Space Flight Center has developed five different lidar for space, and has successfully used them in orbital missions to map Mars, the Earth, the Moon and Mercury. Although similar in some ways, each of these lidar has had a different combination of measurement requirements, payload constraints, and operational environments. Together they have improved space-based lasermeasurement technologies and advanced planetary science. This paper gives a brief overview of these instruments, their measurement approaches and designs, and some highlights from their scientific observations. C1 [Sun, Xiaoli; Abshire, James B.; McGarry, Jan F.; Neumann, Gregory A.; Harding, David J.; Smith, David E.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, James C.; Cavanaugh, John F.] NASA, Instrument Syst & Technol Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zwally, H. Jay] NASA, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci EAPS, Cambridge, MA 02139 USA. RP Sun, XL (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM xiaoli.sun-1@nasa.gov RI Abshire, James/I-2800-2013; Sun, Xiaoli/B-5120-2013; Neumann, Gregory/I-5591-2013; Harding, David/F-5913-2012 OI Neumann, Gregory/0000-0003-0644-9944; NR 62 TC 4 Z9 9 U1 2 U2 24 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1660 EP 1675 DI 10.1109/JSTARS.2013.2259578 PG 16 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800064 ER PT J AU Tsang, L Koh, IS Liao, TH Huang, SW Xu, XL Njoku, EG Kerr, YH AF Tsang, Leung Koh, Il-Suek Liao, Tien-Hao Huang, Shaowu Xu, Xiaolan Njoku, Eni G. Kerr, Yann H. TI Active and Passive Vegetated Surface Models With Rough Surface Boundary Conditions From NMM3D SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Active and passive remote sensings; data cubes; L band; rough surface; tau-omega model ID SOIL-MOISTURE RETRIEVAL; MICROWAVE EMISSION; NUMERICAL-SOLUTIONS; MAXWELL EQUATIONS; SIMULATIONS; SCATTERING AB In this paper, we derive an expression of the brightness temperatures of a vegetated surface based on the tau-omega model with the rough surface boundary condition that replaces the conventional exp(-h) model by NMM3D (Numerical Simulations of 3D Maxwell equations). A purpose of the paper is that the same physical rough surface scattering model based on NMM3D and the same physical paramters of rms heights and correlation lengths can be used for both passive and active remote sensing of the same scene of vegetated surfaces. The bistatic scattering of rough surfaces are decomposed into the coherent wave and the co-polarization and the cross-polarization of the incoherent waves to quantify the contribution of each of these components. Numerical results are illustrated for a variety of roughness conditions. Comparisons are made with the exp(-h) model. Results are compared with the experimental passive measurements of PORTOS 1993 for bare soil cases. Data cubes for grassland are calculated for both active and passive signatures at L band. Comparisons are then made with the L band PALS data for the grassland of SGP99 using these data cubes. C1 [Tsang, Leung; Liao, Tien-Hao; Huang, Shaowu] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. [Koh, Il-Suek] Inha Univ, Dept Elect Engn, Inchon 402451, South Korea. [Xu, Xiaolan; Njoku, Eni G.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Kerr, Yann H.] CESBIO CNES, F-31401 Toulouse, France. RP Tsang, L (reprint author), Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. EM tsang@ee.washington.edu FU NASA/SMAP FX The research was supported by NASA/SMAP. NR 21 TC 8 Z9 8 U1 0 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1698 EP 1709 DI 10.1109/JSTARS.2013.2257694 PG 12 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800067 ER PT J AU Yoon, Y Durand, M Merry, CJ Rodriguez, E AF Yoon, Yeosang Durand, Michael Merry, Carolyn J. Rodriguez, Ernesto TI Improving Temporal Coverage of the SWOT Mission Using Spatiotemporal Kriging SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article; Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS) CY JUL 22-27, 2012 CL Munich, GERMANY SP IEEE, IEEE Geosci & Remote Sensing Soc, DLR, ESA DE Kriging; river height and discharge; SWOT; temporal resolution ID SURFACE-WATER; RIVER; ASSIMILATION; SIMULATION; ALTIMETRY AB The upcoming Surface Water and Ocean Topography (SWOT) satellite mission will measure water surface elevation, its spatial and temporal derivatives, and inundated area. These observations can be used to estimate river discharge at a global scale. SWOT will measure a given area on mid-latitude rivers two or three times per 22-day repeat cycle. In this paper, we suggest an interpolation-based method of estimating water height for times without SWOT observations (i.e., in between SWOT overpasses). A local space-time ordinary kriging (LSTOK) method is developed. Two sets of synthetic SWOT observations are generated by corrupting two different types of true river height with the instrument error. The true river heights are extracted from: 1) simulation of the LISFLOOD-FP hydrodynamic model, and from 2) in situ gage measurements from five USGS gages. Both of these synthetic SWOT observations datasets are important for the following reasons. The model-based dataset provides a complete spatiotemporal picture of river height that is unavailable from in situ measurements, but neglects the effects of e. g. human management actions on river dynamics. On the other hand, the gage-based dataset samples only five locations on the river (1,050 km in length), but represents all effects of human management, tributaries, or other influences on river heights, which are not included in the model. The results are evaluated by a comparison with truth and simple linear interpolation estimates as a first-guess. The model-based experiment shows the LSTOK recovered the river heights with a mean spatial and temporal root mean square error (RMSE) of 11 cm and 12 cm, respectively; these accuracies show a 46% and 54% improvement compared to the RMSEs of the linear interpolation estimates. The gage-based experiment shows a temporal RMSE of 32 cm on average; the LSTOK estimates show a 23% improvement over the linear interpolation estimates. The degradation in performance of the LSTOK for the gage-based analysis as compared to the model-based analysis is apparently due to the effects of human management on river dynamics. Further work is needed to model the effects of human management, and to extend the analysis to consider river tributaries and the main stem of the river simultaneously. C1 [Yoon, Yeosang; Merry, Carolyn J.] Ohio State Univ, Dept Civil Environm & Geodet Engn, Columbus, OH 43210 USA. [Yoon, Yeosang; Durand, Michael; Merry, Carolyn J.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. [Durand, Michael] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Rodriguez, Ernesto] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yoon, Y (reprint author), Ohio State Univ, Dept Civil Environm & Geodet Engn, Columbus, OH 43210 USA. EM yoon.203@osu.edu RI Durand, Michael/D-2885-2013 FU NASA Headquarters under the NASA Earth and Space Science [NNX11AL60H]; NASA Physical Oceanography [NNX10AE96G]; Ohio Supercomputer Center [PAS0503] FX This work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant NNX11AL60H, and the NASA Physical Oceanography grant NNX10AE96G. Computational support for this project was provided by the Ohio Supercomputer Center, under project PAS0503. NR 26 TC 8 Z9 8 U1 1 U2 16 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD JUN PY 2013 VL 6 IS 3 SI SI BP 1719 EP 1729 DI 10.1109/JSTARS.2013.2257697 PG 11 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 170RR UT WOS:000320871800069 ER PT J AU Thompson, DR Bornstein, BJ Chien, SA Schaffer, S Tran, D Bue, BD Castano, R Gleeson, DF Noell, A AF Thompson, David R. Bornstein, Benjamin J. Chien, Steve A. Schaffer, Steven Tran, Daniel Bue, Brian D. Castano, Rebecca Gleeson, Damhnait F. Noell, Aaron TI Autonomous Spectral Discovery and Mapping Onboard the EO-1 Spacecraft SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Endmember detection; hyperspectral imagery; mineralogy; pattern recognition; remote planetary geology; spacecraft autonomy ID IMAGING SPECTROMETER DATA; HYPERSPECTRAL DATA; SCIENCECRAFT EXPERIMENT; ENDMEMBER EXTRACTION; HYPERION; EUROPA; MARS; IDENTIFICATION; SEGMENTATION; COMPRESSION AB Imaging spectrometers are valuable instruments for space exploration, but their large data volumes limit the number of scenes that can be downlinked. Missions could improve science yield by acquiring surplus images and analyzing them onboard the spacecraft. This onboard analysis could generate surficial maps, summarizing scenes in a bandwidth-efficient manner to indicate data cubes that warrant a complete downlink. Additionally, onboard analysis could detect targets of opportunity and trigger immediate automated follow-up measurements by the spacecraft. Here, we report a first step toward these goals with demonstrations of fully automatic hyperspectral scene analysis, feature discovery, and mapping onboard the Earth Observing One (EO-1) spacecraft. We describe a series of overflights in which the spacecraft analyzes a scene and produces summary maps along with lists of salient features for prioritized downlink. The onboard system uses a superpixel endmember detection approach to identify compositionally distinctive features in each image. This procedure suits the limited computing resources of the EO-1 flight processor. It requires very little advance information about the anticipated spectral features, but the resulting surface composition maps agree well with canonical human interpretations. Identical spacecraft commands detect outlier spectral features in multiple scenarios having different constituents and imaging conditions. C1 [Thompson, David R.; Bornstein, Benjamin J.; Chien, Steve A.; Schaffer, Steven; Tran, Daniel; Castano, Rebecca; Gleeson, Damhnait F.; Noell, Aaron] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bue, Brian D.] Rice Univ, Houston, TX 77005 USA. RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM david.r.thompson@jpl.nasa.gov; benjamin.j.bornstein@jpl.nasa.gov; steve.chien@jpl.nasa.gov; steven.r.schaffer@jpl.nasa.gov; daniel.q.tran@jpl.nasa.gov; bbue@rice.edu; rebecca.castano@jpl.nasa.gov; dgleeson@sciops.esa.int; aaron.c.noell@jpl.nasa.gov FU Technology Development Grant under the Advanced Multimission Operating System; National Aeronautics and Space Administration; U.S. Government FX The authors would like to thank the Autonomous Sciencecraft Experiment, the Earth Observing One mission, and the Goddard Space Flight Center (GSFC) for their assistance. The authors would also like to thank the GSFC Science team including E. Middleton, S. Ungar, P. Campbell, and L. Ong. The authors would like to thank D. Mandl and S. Frye for the operations support. The original segmentation methodology was developed by a Technology Development Grant under the Advanced Multimission Operating System and the Multimission Ground Support Services office, with support by J. Wyatt and L. Hall. The authors would like to thank L. Mandrake and M. Gilmore for their help in developing the superpixel segmentation approach. The authors would also like to thank F. Kruse for his assistance and the use of previous work. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. U.S. Government support acknowledged. NR 71 TC 8 Z9 8 U1 1 U2 18 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2013 VL 51 IS 6 BP 3567 EP 3579 DI 10.1109/TGRS.2012.2226040 PN 2 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 171PK UT WOS:000320941300008 ER PT J AU Pasolli, E Melgani, F Alajlan, N Conci, N AF Pasolli, Edoardo Melgani, Farid Alajlan, Naif Conci, Nicola TI Optical Image Classification: A Ground-Truth Design Framework SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Clustering; ground-truth design; hyperspectral; image classification; level set segmentation; support vector machines (SVMs); very high resolution (VHR) ID REMOTELY-SENSED IMAGERY; ACTIVE LEARNING-METHODS; TRAINING DATA; LEVEL SET; SEGMENTATION; ALGORITHMS; SVM AB In the remote sensing field, ground-truth design for collecting training samples represents a tricky and critical problem since it has a direct impact on most of the subsequent image processing and analysis steps. In this paper, we propose a novel framework for assisting a human user in designing ground-truth by photointerpretation for optical remote sensing image classification. The proposed approach is (almost) completely automatic and comprehensive since it aims at assisting the human user from the first to the last step of the process. It is based on unsupervised methods of segmentation and clustering, in order to investigate both the spatial and the spectral information in the process of ground-truth design. The resulting ground-truth is classifier-free and can be further improved by making it classifier-driven through an active learning process. To validate the proposed framework, an experimental study was conducted on very high spatial resolution and hyperspectral images acquired by the IKONOS and the Reflective Optics System Imaging Spectrometer sensors, respectively. The obtained results show the usefulness and effectiveness of the proposed approach. C1 [Pasolli, Edoardo; Melgani, Farid; Conci, Nicola] Univ Trent, Dept Informat Engn & Comp Sci, I-38123 Trento, Italy. [Alajlan, Naif] King Saud Univ, Adv Lab Intelligent Syst Res, Coll Comp & Informat Sci, Riyadh 11543, Saudi Arabia. RP Pasolli, E (reprint author), NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. EM edoardo.pasolli@nasa.gov; melgani@disi.unitn.it; najlan@ksu.edu.sa; conci@disi.unitn.it RI Alajlan, Naif/A-3904-2008; OI Alajlan, Naif/0000-0003-1846-1131; Pasolli, Edoardo/0000-0003-0799-3490 NR 52 TC 7 Z9 7 U1 0 U2 25 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2013 VL 51 IS 6 BP 3580 EP 3597 DI 10.1109/TGRS.2012.2226041 PN 2 PG 18 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 171PK UT WOS:000320941300009 ER PT J AU Moradi, I Meng, H Ferraro, RR Bilanow, S AF Moradi, Isaac Meng, Huan Ferraro, Ralph R. Bilanow, Stephen TI Correcting Geolocation Errors for Microwave Instruments Aboard NOAA Satellites SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Geolocation; microwave remote sensing; navigation; National Oceanic and Atmospheric Administration (NOAA); satellite; satellite tracking ID AMSU-B; PRECIPITABLE WATER; SOUNDING UNIT; SENSOR; RETRIEVAL AB Microwave ( MW) satellite data are widely used as input in numerical weather prediction models and also in other applications such as climate monitoring and re-analysis. MW satellite data are prone to different problems, including geolocation errors. These data do not have a fine spatial resolution like visible and infrared data; therefore, the accuracy of their geolocation cannot be easily determined using the normal methods such as superimposing coastlines on the satellite images. Currently, no geolocation correction is performed on data from MW instruments aboard the satellites in the National Oceanic and Atmospheric Administration ( NOAA) Polar Operational Environmental Satellite program. However, geolocation error can be a significant source of bias in the satellite measurements. In this paper, we investigated and corrected the geolocation errors of the observations from the Advanced Microwave Sounding Unit ( AMSU)-A aboard NOAA-15 to NOAA-19, AMSU-B aboard NOAA-15 to NOAA-17, and Microwave Humidity Sounder ( MHS) aboard NOAA-18 and NOAA-19. We used the difference between ascending and descending observations along the coastlines to quantify the geolocation errors in terms of the satellite attitudes ( Euler angles), i.e., pitch, roll, and yaw. Then, new geographical coordinates and scan/local zenith angles were calculated using new attitudes. The results show that NOAA-15 AMSU-A2 instrument has a mounting error of about 1.2 degrees cross-track, and -0.5 degrees along-track, NOAA-16 AMSU-A1 and -A2 instruments have a mounting error of about -0.5 degrees along-track, and NOAA-18 AMSU-A2 instrument has a mounting error of more than -1 degrees along-track. C1 [Moradi, Isaac] Univ Maryland, Cooperat Inst Climate & Satellites, ESSIC, College Pk, MD 20740 USA. [Meng, Huan; Ferraro, Ralph R.] NOAA, Ctr Satellite Applicat & Res, Natl Environm Satellite Data & Informat Serv, College Pk, MD 20740 USA. [Bilanow, Stephen] NASA, Goddard Space Flight Ctr, Wyle Informat Syst, Greenbelt, MD 20770 USA. RP Moradi, I (reprint author), Univ Maryland, Cooperat Inst Climate & Satellites, ESSIC, College Pk, MD 20740 USA. EM imoradi@umd.edu RI Meng, Huan/F-5613-2010; Ferraro, Ralph/F-5587-2010; Moradi, Isaac/A-7539-2008 OI Meng, Huan/0000-0001-6449-890X; Ferraro, Ralph/0000-0002-8393-7135; Moradi, Isaac/0000-0003-2194-1427 FU National Oceanic and Atmospheric Administration (NOAA)/National Climatic Data Center at the Earth System Science Interdisciplinary Center, University of Maryland [NA09NES4400006] FX Manuscript received March 5, 2012; revised August 7, 2012 and September 18, 2012; accepted October 14, 2012. Date of publication January 22, 2013; date of current version May 16, 2013. This work was supported by the National Oceanic and Atmospheric Administration (NOAA)/National Climatic Data Center under Grant NA09NES4400006 (Cooperative Institute for Climate and Satellites) at the Earth System Science Interdisciplinary Center, University of Maryland. The views, opinions, and findings contained in this report are those of the authors and should not be construed as an official NOAA or U.S. Government position, policy, or decision. NR 21 TC 10 Z9 12 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2013 VL 51 IS 6 BP 3625 EP 3637 DI 10.1109/TGRS.2012.2225840 PN 2 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 171PK UT WOS:000320941300013 ER PT J AU Pellish, JA Galloway, KF AF Pellish, Jonathan A. Galloway, Kenneth F. TI IEEE Nuclear and Space Radiation Effects Conference: Notes on the Early Conferences SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Radiation effects; radiation hardness assurance ID SILICON AB This paper gathers the remembrances of several key contributors who participated in the earliest Institute of Electrical and Electronics Engineers (IEEE) Nuclear and Space Radiation Effects Conferences (NSRECs). C1 [Pellish, Jonathan A.] NASA, Goddard Space Flight Ctr, Flight Data Syst & Radiat Effects Branch, Greenbelt, MD 20771 USA. [Galloway, Kenneth F.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA. RP Pellish, JA (reprint author), NASA, Goddard Space Flight Ctr, Flight Data Syst & Radiat Effects Branch, Greenbelt, MD 20771 USA. EM jonathan.pellish@nasa.gov; ken.galloway@vanderbilt.edu FU NASA Electronic Parts and Packaging Program; Defense Threat Reduction Agency FX This work was supported in part by the NASA Electronic Parts and Packaging Program and the Defense Threat Reduction Agency. NR 12 TC 0 Z9 0 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD JUN PY 2013 VL 60 IS 3 SI SI BP 1681 EP 1689 DI 10.1109/TNS.2013.2262805 PN 2 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 170MU UT WOS:000320857200004 ER PT J AU Xapsos, MA O'Neill, PM O'Brien, TP AF Xapsos, Michael A. O'Neill, Patrick M. O'Brien, T. Paul TI Near-Earth Space Radiation Models SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Galactic cosmic rays; solar particle events; space radiation models; trapped particles ID ENERGETIC PARTICLE EVENTS; SELF-ORGANIZED CRITICALITY; PROTON FLUENCE MODEL; COSMIC-RAY EVENTS; HEAVY-ION MODEL; PROBABILITY MODEL; DOSE FLUCTUATIONS; PEAK FLUXES; SOLAR; ENVIRONMENT AB Review of models of the near-Earth space radiation environment is presented, including recent developments in trapped proton and electron, galactic cosmic ray and solar particle event models geared toward spacecraft electronics applications. C1 [Xapsos, Michael A.; O'Neill, Patrick M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [O'Brien, T. Paul] Aerosp Corp, Chantilly, VA 20151 USA. RP Xapsos, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Michael.A.Xapsos@nasa.gov; Patrick.M.ONeill@nasa.gov; Paul.OBrien@aero.org NR 94 TC 14 Z9 14 U1 0 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD JUN PY 2013 VL 60 IS 3 SI SI BP 1691 EP 1705 DI 10.1109/TNS.2012.2225846 PN 2 PG 15 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 170MU UT WOS:000320857200005 ER PT J AU Reed, RA Weller, RA Akkerman, A Barak, J Culpepper, W Duzellier, S Foster, C Gaillardin, M Hubert, G Jordan, T Jun, I Koontz, S Lei, F McNulty, P Mendenhall, MH Murat, M Nieminen, P O'Neill, P Raine, M Reddell, B Saigne, F Santin, G Sihver, L Tang, HHK Truscott, PR Wrobel, F AF Reed, R. A. Weller, R. A. Akkerman, A. Barak, J. Culpepper, W. Duzellier, S. Foster, C. Gaillardin, M. Hubert, G. Jordan, T. Jun, I. Koontz, S. Lei, F. McNulty, P. Mendenhall, M. H. Murat, M. Nieminen, P. O'Neill, P. Raine, M. Reddell, B. Saigne, F. Santin, G. Sihver, L. Tang, H. H. K. Truscott, P. R. Wrobel, F. TI Anthology of the Development of Radiation Transport Tools as Applied to Single Event Effects SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Monte Carlo radiation transport; single event effects ID NEUTRON-INDUCED SEU; MONTE-CARLO CALCULATIONS; INDUCED SOFT ERRORS; ACCURATE UNIVERSAL PARAMETERIZATION; ABSORPTION CROSS-SECTIONS; INDUCED NUCLEAR-REACTIONS; HEAVY-ION TRANSPORT; MICRODOSIMETRIC KINETIC-MODEL; TERRESTRIAL COSMIC-RAYS; UPSET RATE PREDICTION AB This anthology contains contributions from eleven different groups, each developing and/or applying Monte Carlo-based radiation transport tools to simulate a variety of effects that result from energy transferred to a semiconductor material by a single particle event. The topics span from basic mechanisms for single-particle induced failures to applied tasks like developing websites to predict on-orbit single event failure rates using Monte Carlo radiation transport tools. C1 [Reed, R. A.; Weller, R. A.; Mendenhall, M. H.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37212 USA. [Reed, R. A.; Weller, R. A.; Mendenhall, M. H.] Vanderbilt Univ, Inst Space & Def Elect, Nashville, TN 37212 USA. [Akkerman, A.; Barak, J.; Murat, M.] Soreq NRC, IL-81800 Yavne, Israel. [Duzellier, S.; Hubert, G.] French Aerosp Lab ONERA, F-31055 Toulouse, France. [Gaillardin, M.; Raine, M.] CEA, DAM, DIF, F-91297 Arpajon, France. [Jordan, T.] EMP Consultants, Gaithersburg, MD 20885 USA. [Jun, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Culpepper, W.; Foster, C.; Koontz, S.; O'Neill, P.; Reddell, B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [McNulty, P.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Nieminen, P.; Santin, G.] ESA ESTEC, Space Environments & Effects Sect TOS EES, NL-2200 AG Noordwijk, Netherlands. [Saigne, F.; Wrobel, F.] Univ Montpellier 2, F-34095 Montpellier 5, France. [Santin, G.] Rhea Syst SA, B-1348 Louvain, Belgium. [Sihver, L.] Chalmers, S-41296 Gothenburg, Sweden. [Sihver, L.] Roanoke Coll, Salem, VA 24153 USA. [Sihver, L.] Texas A&M Univ, College Stn, TX 77843 USA. [Truscott, P. R.] Kallisto Consultancy Ltd, Yorktown Hts, NY 10598 USA. RP Reed, RA (reprint author), Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37212 USA. EM robert.reed@vanderbilt.edu RI Reed, Robert/N-1988-2013; Raine, Melanie/F-6357-2011 OI Raine, Melanie/0000-0002-1898-9473 NR 276 TC 21 Z9 21 U1 0 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD JUN PY 2013 VL 60 IS 3 SI SI BP 1876 EP 1911 DI 10.1109/TNS.2013.2262101 PN 2 PG 36 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 170MU UT WOS:000320857200015 ER PT J AU Adell, PC Scheick, LZ AF Adell, P. C. Scheick, L. Z. TI Radiation Effects in Power Systems: A Review SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE DC-DC converters; digital control; linear regulators; power systems; single event effects; total dose ID SINGLE-EVENT TRANSIENTS; LINEAR VOLTAGE REGULATORS; DOSE-RATE; OPERATIONAL-AMPLIFIER; PROTON IRRADIATION; IONIZING-RADIATION; ANGULAR-DEPENDENCE; CIRCUIT RESPONSE; GATE-RUPTURE; HEAVY-ION AB To guarantee mission success and minimize the risk of anomalies in space, current space-power architectures are designed conservatively and use electronics that are several generations behind the current state of the art. In parallel, the commercial industry is burgeoning with exciting new solutions for power management; however, their reliability and radiation robustness for space application have yet to be proven. The goal of this paper is to review common radiation issues related to power converters, which are the main design blocks of current space power system architectures. We first provide some background material and introduce the basic principles of power converter operation, as well as a brief introduction of common radiation effect that might damage these designs. Then, we explain common radiation-induced failure mechanisms (radiation-induced failure or instability) or temporary perturbations observed in various converter topologies. Their radiation hardness is compared based on simulation and experimental studies reported in the literature. Some radiation hardening by design solutions and mitigation techniques are also presented. Finally, we provide a status of emerging technologies under consideration for the next-generation of space power systems. C1 [Adell, P. C.; Scheick, L. Z.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Adell, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM philippe.c.adell@jpl.nasa.gov FU NASA Electronic Parts and Packaging Program; National Reconnaissance Office, Vanderbilt University; Jet Propulsion Laboratory, California Institute of Technology FX The authors would like to thank the NASA Electronic Parts and Packaging Program, the National Reconnaissance Office, Vanderbilt University and Jet Propulsion Laboratory, California Institute of Technology research and development funds for having supported this research into radiation effects in power systems over many years. NR 78 TC 12 Z9 12 U1 3 U2 22 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD JUN PY 2013 VL 60 IS 3 SI SI BP 1929 EP 1952 DI 10.1109/TNS.2013.2262235 PN 2 PG 24 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 170MU UT WOS:000320857200017 ER PT J AU Gerardin, S Bagatin, M Paccagnella, A Grurmann, K Gliem, F Oldham, TR Irom, F Nguyen, DN AF Gerardin, S. Bagatin, M. Paccagnella, A. Gruermann, K. Gliem, F. Oldham, T. R. Irom, F. Nguyen, D. N. TI Radiation Effects in Flash Memories SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Flash memories; floating gate (FG); single event functional interrupts (SEFI); single event upset (SEU); soft errors ID FLOATING-GATE MEMORIES; HEAVY-ION IRRADIATION; CHARGE LOSS; MOSFET DOSIMETER; COMMERCIAL NAND; SIO2 LAYERS; CELLS; EXPOSURE; ARRAYS; RELIABILITY AB We review ionizing radiation effects in Flash memories, the current dominant technology in the commercial non-volatile memory market. A comprehensive discussion of total dose and single event effects results is presented, concerning both floating gate cells and peripheral circuitry. The latest developments, including new findings on the mechanism underlying upsets due to heavy ions and destructive events, are illustrated. C1 [Gerardin, S.; Bagatin, M.; Paccagnella, A.] Univ Padua, Dipartimento Ingn Informaz, RREACT Grp, I-35131 Padua, Italy. [Bagatin, M.; Paccagnella, A.] Ist Nazl Fis Nucl INFN, I-35131 Padua, Italy. [Gruermann, K.; Gliem, F.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Comp & Network Engn, IDA, D-38106 Braunschweig, Germany. [Oldham, T. R.] Ball Aerosp Technol Ctr, Boulder, CO 80301 USA. [Irom, F.; Nguyen, D. N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gerardin, S (reprint author), Univ Padua, Dipartimento Ingn Informaz, RREACT Grp, I-35131 Padua, Italy. EM simone.ger-ardin@dei.unipdit; marta.bagatin@dei.unipd.it; alessandro.paccagnella@dei.unipd.it; toldham@ball.com NR 82 TC 39 Z9 39 U1 4 U2 34 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD JUN PY 2013 VL 60 IS 3 SI SI BP 1953 EP 1969 DI 10.1109/TNS.2013.2254497 PN 2 PG 17 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 170MU UT WOS:000320857200018 ER PT J AU Johnston, AH AF Johnston, Allan H. TI Radiation Effects in Optoelectronic Devices SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Detectors; laser diodes; light-emitting diodes; optoelectronics; radiation effects ID LIGHT-EMITTING-DIODES; DISPLACEMENT DAMAGE; ENERGY-DEPENDENCE; PROTON DAMAGE; LASER-DIODES; HARDNESS ASSURANCE; SILICON DEVICES; COSMIC-RAYS; IRRADIATED SILICON; CARRIER REMOVAL AB This review paper discusses radiation effects in a variety of optoelectronic devices. The main emphasis is on displacement and total dose damage under conditions that are representative of various space missions. However, the mechanisms for degradation in space are also applicable to other environments, such as nuclear reactors, and the extremely high-energy particles associated with the Large Hadron Collider at CERN. In addition to permanent damage effects, there is also an abbreviated treatment of single-event effects in optoelectronic devices. 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 NR 107 TC 13 Z9 13 U1 2 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD JUN PY 2013 VL 60 IS 3 SI SI BP 2054 EP 2073 DI 10.1109/TNS.2013.2259504 PN 2 PG 20 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 170MU UT WOS:000320857200023 ER PT J AU Ahmed, R Siqueira, P Hensley, S Bergen, K AF Ahmed, Razi Siqueira, Paul Hensley, Scott Bergen, Kathleen TI Uncertainty of Forest Biomass Estimates in North Temperate Forests Due to Allometry: Implications for Remote Sensing SO REMOTE SENSING LA English DT Article DE biomass; allometry; uncertainty; Harvard forest; Howland forest AB Estimates of above ground biomass density in forests are crucial for refining global climate models and understanding climate change. Although data from field studies can be aggregated to estimate carbon stocks on global scales, the sparsity of such field data, temporal heterogeneity and methodological variations introduce large errors. Remote sensing measurements from spaceborne sensors are a realistic alternative for global carbon accounting; however, the uncertainty of such measurements is not well known and remains an active area of research. This article describes an effort to collect field data at the Harvard and Howland Forest sites, set in the temperate forests of the Northeastern United States in an attempt to establish ground truth forest biomass for calibration of remote sensing measurements. We present an assessment of the quality of ground truth biomass estimates derived from three different sets of diameter-based allometric equations over the Harvard and Howland Forests to establish the contribution of errors in ground truth data to the error in biomass estimates from remote sensing measurements. C1 [Ahmed, Razi; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Siqueira, Paul] Univ Massachusetts, Coll Engn, Amherst, MA 01002 USA. [Bergen, Kathleen] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. RP Ahmed, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM razi.u.ahmed@jpl.nasa.gov; siqueira@ecs.umass.edu; scott.hensley@jpl.nasa.gov; kbergen@umich.edu FU National Aeronautics and Space Administration; NASA [NNX09AI18G]; NASA's Terrestrial Ecology program FX Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research was supported by NASA under the Terrestrial Ecology grant NNX09AI18G. The authors would like to express appreciation to the Harvard Forest who facilitated much of the ground validation work described here. Field data for the Howland Research Forest and Harvard Forest was acquired through the DESDynI field campaign, also funded by NASA's Terrestrial Ecology program. NR 5 TC 9 Z9 12 U1 1 U2 37 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2013 VL 5 IS 6 BP 3007 EP 3036 DI 10.3390/rs5063007 PG 30 WC Remote Sensing SC Remote Sensing GA 169HP UT WOS:000320771100020 ER PT J AU Quinn, RC Martucci, HFH Miller, SR Bryson, CE Grunthaner, FJ Grunthaner, PJ AF Quinn, Richard C. Martucci, Hana F. H. Miller, Stephanie R. Bryson, Charles E. Grunthaner, Frank J. Grunthaner, Paula J. TI Perchlorate Radiolysis on Mars and the Origin of Martian Soil Reactivity SO ASTROBIOLOGY LA English DT Article DE Mars; Radiolysis; Organic degradation; in situ measurement; Planetary habitability and biosignatures ID GAS-EXCHANGE EXPERIMENT; VIKING; MODEL; CHEMISTRY; PRODUCT; SIMULATIONS AB Results from the Viking biology experiments indicate the presence of reactive oxidants in martian soils that have previously been attributed to peroxide and superoxide. Instruments on the Mars Phoenix Lander and the Mars Science Laboratory detected perchlorate in martian soil, which is nonreactive under the conditions of the Viking biology experiments. We show that calcium perchlorate exposed to gamma rays decomposes in a CO2 atmosphere to form hypochlorite (ClO-), trapped oxygen (O-2), and chlorine dioxide (ClO2). Our results show that the release of trapped O-2 (g) from radiation-damaged perchlorate salts and the reaction of ClO- with amino acids that were added to the martian soils can explain the results of the Viking biology experiments. We conclude that neither hydrogen peroxide nor superoxide is required to explain the results of the Viking biology experiments. C1 [Quinn, Richard C.] NASA, Ames Res Ctr, Carl Sagan Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Martucci, Hana F. H.] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA. [Miller, Stephanie R.] NASA, Ames Educ Associates Program, Moffett Field, CA USA. [Bryson, Charles E.] Apparati Inc, Mountain View, CA USA. [Grunthaner, Frank J.; Grunthaner, Paula J.] NASA, Jet Prop Lab, Pasadena, CA USA. RP Quinn, RC (reprint author), NASA, Ames Res Ctr, Carl Sagan Ctr, SETI Inst, MS 239-4, Moffett Field, CA 94035 USA. EM Richard.C.Quinn@nasa.gov FU NASA [NNX09AM93G] FX Funding was provided by the NASA Astrobiology: Exobiology and Evolutionary Biology Program (grant NNX09AM93G). The authors thank C.P. McKay, C.R. Stoker and Inge ten Kate for their reviews and comments. The authors also acknowledge Dr. Cynthia B. Phillips (SETI Institute) and Dr. Monika Kress (SJSU). Partial funding for H. Martucci was provided by the NASA Education and Public Outreach in Earth and Space Science (EPOESS) program. NR 32 TC 29 Z9 29 U1 4 U2 49 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2013 VL 13 IS 6 BP 515 EP 520 DI 10.1089/ast.2013.0999 PG 6 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 168LO UT WOS:000320707500001 PM 23746165 ER PT J AU Lomeli, MJM Wakefield, WW AF Lomeli, Mark J. M. Wakefield, W. Waldo TI A flexible sorting grid to reduce Pacific halibut (Hippoglossus stenolepis) bycatch in the US west coast groundfish bottom trawl fishery SO FISHERIES RESEARCH LA English DT Article DE Bycatch reduction device; Flexible sorting grid; Pacific halibut; Bottom trawl ID SELECTIVE FLATFISH TRAWL; HERDING BEHAVIOR; SIZE SELECTION; DIEL VARIATION; DEVICES BRDS; NORTH-SEA; ROCKFISH; NIGHT; CATCHABILITY; MERLUCCIUS AB This study examined a flexible sorting grid excluder designed to reduce Pacific halibut (Hippoglossus stenolepis) bycatch in the US west coast groundfish bottom trawl fishery. Tests occurred off Washington during 2011 aboard a commercial trawler. A recapture net was used to quantify the retention rates of target and non-target species. Pacific halibut bycatch was reduced 61.6% by weight and 57.0% by numbers. Exclusion was greatest for Pacific halibut weighing more than 4.5 kg. A significant difference in the mean total length was also noted between Pacific halibut caught in the codend and the recapture net, with larger fish occurring in the recapture net. The retention of primary target groundfishes of marketable-size ranged from 76.7 to 89.3%. We demonstrated the capability of a flexible sorting grid excluder to reduce Pacific halibut bycatch in the groundfish bottom trawl fishery while retaining a relatively high proportion of the targeted species. (C) 2013 Elsevier B.V. All rights reserved. C1 [Lomeli, Mark J. M.] Pacific States Marine Fisheries Commiss, Newport, OR 97365 USA. [Wakefield, W. Waldo] Natl Ocean & Atmospher Adm, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Lomeli, MJM (reprint author), Pacific States Marine Fisheries Commiss, 2032 SE OSU Dr, Newport, OR 97365 USA. EM mlomeli@psmfc.org FU NOAA National Marine Fisheries Service Bycatch Reduction Engineering Program FX We would like to thank the captain and crew of the F/V Miss Leona for their assistance with this research. We would also like to thank Craig Rose (NOAA Fisheries-Alaska Fisheries Science Center), John Gauvin (Gauvin and Associates), and Dantrawl Inc. as they played important roles in developing this project, Andi Stephens (NOM Fisheries-Northwest Fisheries Science Center) for assisting with the GLMM analysis, and the internal (Jason Jannot, NOAA Fisheries-Northwest Fisheries Science Center) and external reviewers who critically reviewed and contributed to this manuscript. Funding for this study was provided by NOAA National Marine Fisheries Service Bycatch Reduction Engineering Program. NR 29 TC 3 Z9 3 U1 0 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 J9 FISH RES JI Fish Res. PD JUN PY 2013 VL 143 BP 102 EP 108 DI 10.1016/j.fishres.2013.01.017 PG 7 WC Fisheries SC Fisheries GA 151WS UT WOS:000319491700011 ER PT J AU Shebalin, JV AF Shebalin, John V. TI Broken ergodicity, magnetic helicity, and the MHD dynamo SO GEOPHYSICAL AND ASTROPHYSICAL FLUID DYNAMICS LA English DT Article DE Magnetohydrodynamics; Turbulence; Statistical Mechanics; Dynamo theory ID MAGNETOHYDRODYNAMIC TURBULENCE; FIELD AB We consider an unforced, incompressible, turbulent magnetofluid constrained by concentric inner and outer spherical surfaces. We define a model system in which normal components of the velocity, magnetic field, vorticity, and electric current are zero on the boundaries. This choice allows us to find a set of Galerkin expansion functions that are common to both velocity and magnetic field, as well as vorticity and current. The model dynamical system represents magnetohydrodynamic (MHD) turbulence in a spherical domain and is analyzed by the methods similar to those applied to homogeneous MHD turbulence. We find a statistical theory of ideal (i.e. no dissipation) MHD turbulence analogous to that found in the homogeneous case, including the prediction of coherent structure in the form of a large-scale quasistationary magnetic field. This MHD dynamo depends on broken ergodicity, an effect that is enhanced when total magnetic helicity is increased relative to total energy. When dissipation is added and large scales are only weakly damped, quasiequilibrium may occur for long periods of time, so that the ideal theory is still pertinent on a global scale. Over longer periods of time, the selective decay of energy over magnetic helicity further enhances the effects of broken ergodicity. Thus, broken ergodicity is an essential mechanism and relative magnetic helicity is a critical parameter in this model MHD dynamo theory. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Shebalin, JV (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM john.v.shebalin@nasa.gov NR 42 TC 4 Z9 4 U1 0 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0309-1929 EI 1029-0419 J9 GEOPHYS ASTRO FLUID JI Geophys. Astrophys. Fluid Dyn. PD JUN 1 PY 2013 VL 107 IS 3 BP 353 EP 375 DI 10.1080/03091929.2012.689299 PG 23 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Mechanics SC Astronomy & Astrophysics; Geochemistry & Geophysics; Mechanics GA 166RU UT WOS:000320575600005 ER PT J AU Wong, WC Zalesak, S Yoets, A Capriotti, J Smith, MJ Castro, VA Pierson, DL AF Wong, Wing C. Zalesak, Selina Yoets, Airan Capriotti, Jason Smith, Melanie J. Castro, Victoria A. Pierson, Duane L. TI Engineering Case Report: Effectiveness of HEPA Filter Vacuum in Removing Transient Microbial Contaminants on Cargo Bags Destined for the International Space Station SO JOURNAL OF OCCUPATIONAL AND ENVIRONMENTAL HYGIENE LA English DT Article C1 [Wong, Wing C.; Yoets, Airan; Smith, Melanie J.; Castro, Victoria A.] Enterprise Advisory Serv, Houston, TX USA. [Zalesak, Selina] Univ Space Res Assoc, Houston, TX USA. [Wong, Wing C.; Capriotti, Jason] NIST, Gaithersburg, MD 20899 USA. [Pierson, Duane L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Wong, WC (reprint author), NIST, 100 Bur Dr, Gaithersburg, MD 20899 USA. EM wing.wong@nist.gov FU NASA ISS [NAS9-02078] FX The authors thank Rebekah Bruce and Thomas Molina of the Microbiology Laboratory at NASA Johnson Space Center for their assistance in this study. This study was supported by NASA ISS funding NAS9-02078. NR 8 TC 0 Z9 0 U1 1 U2 5 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1545-9624 J9 J OCCUP ENVIRON HYG JI J. Occup. Environ. Hyg. PD JUN 1 PY 2013 VL 10 IS 6 BP D71 EP D75 DI 10.1080/15459624.2013.784179 PG 5 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA 172DL UT WOS:000320980100002 PM 23621341 ER PT J AU Benafan, O Padula, SA Noebe, RD Brown, DW Clausen, B Vaidyanathan, R AF Benafan, O. Padula, S. A., II Noebe, R. D. Brown, D. W. Clausen, B. Vaidyanathan, R. TI An in situ neutron diffraction study of shape setting shape memory NiTi SO ACTA MATERIALIA LA English DT Article DE NiTi; Shape setting; Neutron diffraction; Blocking stress; Stress relaxation ID CONSTRAINED PHASE-TRANSFORMATION; MARTENSITIC-TRANSFORMATION; RIETVELD REFINEMENT; STRESS-RELAXATION; TEXTURE ANALYSIS; RECOVERY STRESS; ALLOYS; STRAIN; BEHAVIOR; DEFORMATION AB A bulk polycrystalline Ni49.9Ti50.1 (at.%) shape memory alloy specimen was shape set while neutron diffraction spectra were simultaneously acquired. The objective was to correlate internal stress, phase volume fraction, and texture measurements (from neutron diffraction spectra) with the macroscopic stress and shape changes (from load cell and extensometry measurements) during the shape setting procedure and subsequent shape recovery. Experimental results showed the evolution of the martensitic transformation (lattice strains, phase fractions and texture) against external constraints during both heating and cooling. Constrained heating resulted in a build-up of stresses during the martensite to austenite transformation, followed by stress relaxation due to thermal expansion, final conversion of retained martensite, and recovery processes. Constrained cooling also resulted in stress build-up arising from thermal contraction and early formation of martensite, followed by relaxation as the austenite fully transformed to martensite. Comparisons were also made between specimens pre-shape set and post-shape set with and without external constraints. The specimens displayed similar shape memory behavior consistent with the microstructure of the shape set sample, which was mostly unchanged by the shape setting process and similar to that of the as-received material. Published by Elsevier Ltd. on behalf of Acta Materialia Inc. C1 [Benafan, O.; Vaidyanathan, R.] Univ Cent Florida, Adv Mat Proc & Anal Ctr, Mat & Aerosp Engn Dept, Orlando, FL 32816 USA. [Benafan, O.; Padula, S. A., II; Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Brown, D. W.; Clausen, B.] Los Alamos Natl Lab, Lujan Ctr, Los Alamos, NM 87545 USA. RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM othmane.benafan@nasa.gov RI Clausen, Bjorn/B-3618-2015 OI Clausen, Bjorn/0000-0003-3906-846X FU NASA Fundamental Aeronautics Program; Aeronautical Sciences Project; Office of Basic Energy Sciences DOE; DOE [DE-AC52-06NA25396] FX Funding from the NASA Fundamental Aeronautics Program, Aeronautical Sciences Project is gratefully acknowledged. The authors thank T.A. Sisneros at LANL, and D. Gaydosh, G. Bigelow and A. Garg at NASA GRC for technical support and helpful discussions. The authors also thank S. Qiu and D.E. Nicholson from UCF for their help in performing the neutron diffraction experiments. This work has benefited from the use of the Lujan Neutron Scattering Center at LANSCE, which is funded by the Office of Basic Energy Sciences DOE. LANL is operated by Los Alamos National Security LLC under DOE Contract No. DE-AC52-06NA25396. NR 49 TC 13 Z9 14 U1 2 U2 37 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 EI 1873-2453 J9 ACTA MATER JI Acta Mater. PD JUN PY 2013 VL 61 IS 10 BP 3585 EP 3599 DI 10.1016/j.actamat.2013.02.040 PG 15 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 149FM UT WOS:000319304400005 ER PT J AU Lee, CP Anilkumar, AV Cox, MC Lioi, CB Grugel, RN AF Lee, C. P. Anilkumar, A. V. Cox, M. C. Lioi, C. B. Grugel, R. N. TI Evolution of elongated pores at the melt-solid interface during controlled directional solidification SO ACTA MATERIALIA LA English DT Article DE Gasarite; Eutectic; Pore formation; Directional solidification; Jackson-Hunt equation ID GASARITE EUTECTIC GROWTH; FABRICATION AB The evolution of elongated gaseous pores during directional solidification has been examined through a theoretical model and compared to previous experimental findings from the literature. The model is based on the observation and interpretation of a wedge-shaped structure on the solid side that extends beyond the melt solid interface and wraps around the bubble at its equator. At the tip of the wedge is the meeting point of the melt, solid and gas. The model takes into account the competition around the meeting point between the law of segregation of the solute at the melt solid interface on one hand, and Henry's law, which governs the concentration of the solute at the melt-pore interface at a given pressure, on the other. It predicts VR2 = constant, where V is the processing speed and R is the pore radius, and agrees well with reported experimental data. Published by Elsevier Ltd. on behalf of Acta Materialia Inc. C1 [Lee, C. P.] Craft Tech Inc, Huntsville, AL 35801 USA. [Anilkumar, A. V.; Cox, M. C.; Lioi, C. B.] Vanderbilt Univ, Dept Mech Engn, Nashville, TN 37235 USA. [Grugel, R. N.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Grugel, RN (reprint author), NASA, George C Marshall Space Flight Ctr, EM 30, Huntsville, AL 35812 USA. EM Richard.N.Grugel@nasa.gov NR 12 TC 3 Z9 3 U1 0 U2 17 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 JUN PY 2013 VL 61 IS 10 BP 3752 EP 3757 DI 10.1016/j.actamat.2013.03.006 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 149FM UT WOS:000319304400020 ER PT J AU Barth, AJ Pancoast, A Bennert, VN Brewer, BJ Canalizo, G Filippenko, AV Gates, EL Greene, JE Li, WD Malkan, MA Sand, DJ Stern, D Treu, T Woo, JH Assef, RJ Bae, HJ Buehler, T Cenko, SB Clubb, KI Cooper, MC Diamond-Stanic, AM Honig, SF Joner, MD Laney, CD Lazarova, MS Nierenberg, AM Silverman, JM Tollerud, EJ Walsh, JL AF Barth, Aaron J. Pancoast, Anna Bennert, Vardha N. Brewer, Brendon J. Canalizo, Gabriela Filippenko, Alexei V. Gates, Elinor L. Greene, Jenny E. Li, Weidong Malkan, Matthew A. Sand, David J. Stern, Daniel Treu, Tommaso Woo, Jong-Hak Assef, Roberto J. Bae, Hyun-Jin Buehler, Tabitha Cenko, S. Bradley Clubb, Kelsey I. Cooper, Michael C. Diamond-Stanic, Aleksandar M. Hoenig, Sebastian F. Joner, Michael D. Laney, C. David Lazarova, Mariana S. Nierenberg, A. M. Silverman, Jeffrey M. Tollerud, Erik J. Walsh, Jonelle L. TI THE LICK AGN MONITORING PROJECT 2011: Fe II REVERBERATION FROM THE OUTER BROAD-LINE REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Mrk 1511, NGC 4593); galaxies: nuclei ID ACTIVE GALACTIC NUCLEI; VELOCITY-DELAY MAPS; SEYFERT 1 GALAXIES; BLACK-HOLE MASSES; IMAGE SUBTRACTION; EMISSION FEATURES; CORRELATION SPACE; ARP 151; QUASARS; VARIABILITY AB The prominent broad Fe II emission blends in the spectra of active galactic nuclei have been shown to vary in response to continuum variations, but past attempts to measure the reverberation lag time of the optical Fe II lines have met with only limited success. Here we report the detection of Fe II reverberation in two Seyfert 1 galaxies, NGC 4593 and Mrk 1511, based on data from a program carried out at Lick Observatory in Spring 2011. Light curves for emission lines including H beta and Fe II were measured by applying a fitting routine to decompose the spectra into several continuum and emission-line components, and we use cross-correlation techniques to determine the reverberation lags of the emission lines relative to V-band light curves. In both cases, the measured lag (tau(cen)) of Fe II is longer than that of H beta, although the inferred lags are somewhat sensitive to the choice of Fe II template used in the fit. For spectral decompositions done using the Fe II template of Veron-Cetty et al., we find tau(cen)(Fe II)/tau(cen)(H beta) = 1.9 +/- 0.6 in NGC 4593 and 1.5 +/- 0.3 in Mrk 1511. The detection of highly correlated variations between Fe II and continuum emission demonstrates that the Fe II emission in these galaxies originates in photoionized gas, located predominantly in the outer portion of the broad-line region. C1 [Barth, Aaron J.; Cooper, Michael C.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Pancoast, Anna; Treu, Tommaso; Hoenig, Sebastian F.; Nierenberg, A. M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bennert, Vardha N.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA. [Brewer, Brendon J.] Univ Auckland, Dept Stat, Auckland 1142, New Zealand. [Canalizo, Gabriela; Lazarova, Mariana S.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Filippenko, Alexei V.; Li, Weidong; Cenko, S. Bradley; Clubb, Kelsey I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Gates, Elinor L.] Univ Calif Santa Cruz, Lick Observ, Mt Hamilton, CA 95140 USA. [Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Malkan, Matthew A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Sand, David J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Woo, Jong-Hak] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. [Bae, Hyun-Jin] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Bae, Hyun-Jin] Yonsei Univ, Ctr Galaxy Evolut Res, Seoul 120749, South Korea. [Buehler, Tabitha] Brigham Young Univ, Dept Phys & Astron, ESC N283, Provo, UT 84602 USA. [Diamond-Stanic, Aleksandar M.] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Lazarova, Mariana S.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Tollerud, Erik J.] Yale Univ, Dept Astron, New Haven, CT 06510 USA. RP Barth, AJ (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. EM barth@uci.edu RI Woo, Jong-Hak/A-2790-2014; Bae, Hyun-Jin/J-8037-2015; OI Bae, Hyun-Jin/0000-0001-5134-5517; Tollerud, Erik/0000-0002-9599-310X; Hoenig, Sebastian/0000-0002-6353-1111; Barth, Aaron/0000-0002-3026-0562 FU NSF [AST-110812, 1107865, 1108665, 1108835, AST-1211916, AST-1102845, AST-0618209]; Gary & Cynthia Bengier; Richard & Rhoda Goldman Fund; TABASGO Foundation; Christopher R. Redlich Fund; Packard Research Fellowship; NASA; National Research Foundation of Korea (NRF); Korea government (MEST) [2012-006087] FX We are extremely grateful to the Lick Observatory staff for their outstanding assistance during our 2011 observing run. The Lick AGN Monitoring Project 2011 is supported by NSF grants AST-110812, 1107865, 1108665, and 1108835. A. P. acknowledges support from the NSF through the Graduate Research Fellowship Program. A.V.F.'s group at UC Berkeley received additional funding through NSF grant AST-1211916, Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the TABASGO Foundation, and the Christopher R. Redlich Fund. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. T. T. acknowledges a Packard Research Fellowship. The work of D. S. and R.J.A. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Research by J.L.W. is supported by NSF grant AST-1102845. J.H.W. acknowledges support by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MEST; No. 2012-006087). The West Mountain Observatory receives support from NSF grant AST-0618209. We thank the anonymous referee for helpful suggestions. We mourn the tragic passing of our friend and collaborator, Weidong Li, who devotedly oversaw the nightly operation of KAIT and taught us much about photometry. This work is dedicated to the memory of Lick Observatory staff member Greg Sulger. NR 81 TC 43 Z9 43 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2013 VL 769 IS 2 AR UNSP 128 DI 10.1088/0004-637X/769/2/128 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100044 ER PT J AU Boersma, C Bregman, JD Allamandola, LJ AF Boersma, C. Bregman, J. D. Allamandola, L. J. TI PROPERTIES OF POLYCYCLIC AROMATIC HYDROCARBONS IN THE NORTHWEST PHOTON DOMINATED REGION OF NGC 7023. I. PAH SIZE, CHARGE, COMPOSITION, AND STRUCTURE DISTRIBUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: individual objects (NGC 7023); molecular data; techniques: spectroscopic ID INFRARED-EMISSION SPECTRA; BLIND SIGNAL SEPARATION; SPITZER-SPACE-TELESCOPE; REFLECTION NEBULAE; CARBON GRAINS; PHOTODISSOCIATION REGIONS; SPECTROSCOPIC DATABASE; INTERSTELLAR DUST; AMORPHOUS-CARBON; FEATURES AB Polycyclic aromatic hydrocarbon (PAH) emission in the Spitzer Infrared Spectrograph spectral map of the northwest photon dominated region (PDR) in NGC 7023 was analyzed exclusively using PAH spectra from the NASA Ames PAH IR Spectroscopic Database (www.astrochem.org/pahdb). The 5-15 mu m spectrum at each pixel is fitted using a non-negative-least-squares fitting approach. The fits are of good quality, allowing decomposition of the PAH emission into four subclasses: size, charge, composition, and hydrogen adjacency (structure). Maps tracing PAH subclass distributions across the region paint a coherent astrophysical picture. Once past some 20 seconds of arc from HD 200775, the emission is dominated by the more stable, large, symmetric, compact PAH cations with smaller, neutral PAHs taking over along the lines-of-sight toward the more distant molecular cloud. The boundary between the PDR and the denser cloud material shows up as a distinct discontinuity in the breakdown maps. Noteworthy is the requirement for PANH cations to fit the bulk of the 6.2 and 11.0 mu m features and the indication of PAH photo-dehydrogenation and fragmentation close to HD 200775. Decomposition of the spectral maps into "principal" subclass template spectra provides additional insight into the behavior of each subclass. However, the general applicability of this computationally more efficient approach is presently undetermined. This is the first time the spectra of individual PAHs are exclusively used to fit the 5-15 mu m region and analyze the spatial behavior of the aromatic infrared bands, providing fundamental, new information about astronomical PAH subpopulations including their dependence on, and response to, changes in local conditions. C1 [Boersma, C.; Bregman, J. D.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Boersma, C (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM Christiaan.Boersma@nasa.gov RI Boersma, Christiaan/L-7696-2014 OI Boersma, Christiaan/0000-0002-4836-217X FU NASA [1407]; NASA's Laboratory Astrophysics; "Carbon in the Galaxy" consortium [NNH10ZDA001N]; NASA's Astrobiology; Astronomy + Physics Research and Analysis (APRA) [NNX07AH02G]; Spitzer Space Telescope Support Programs [50082]; San Jose State University Research Foundation [NNX11AJ33A] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support from NASA's Laboratory Astrophysics, "Carbon in the Galaxy" consortium grant (NNH10ZDA001N); and NASA's Astrobiology; Astronomy + Physics Research and Analysis (APRA; NNX07AH02G), and Spitzer Space Telescope Support Programs (50082) are greatly acknowledged. C. B. is especially grateful for appointments to the NASA Post-doctoral Program at the Ames Research Center administered by Oak Ridge Associated Universities through a contract with NASA and by San Jose State University Research Foundation (grant NNX11AJ33A). Lastly, the careful reading and helpful suggestions made by an anonymous referee are acknowledged. NR 71 TC 31 Z9 31 U1 0 U2 22 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 JUN 1 PY 2013 VL 769 IS 2 AR UNSP 117 DI 10.1088/0004-637X/769/2/117 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100033 ER PT J AU Bridge, CR Blain, A Borys, CJK Petty, S Benford, D Eisenhardt, P Farrah, D Griffith, RL Jarrett, T Lonsdale, C Stanford, SA Stern, D Tsai, CW Wright, EL Wu, JW AF Bridge, Carrie R. Blain, Andrew Borys, Colin J. K. Petty, Sara Benford, Dominic Eisenhardt, Peter Farrah, Duncan Griffith, Roger L. Jarrett, Tom Lonsdale, Carol Stanford, Spencer A. Stern, Daniel Tsai, Chao-Wei Wright, Edward L. Wu, Jingwen TI A NEW POPULATION OF HIGH-z, DUSTY Ly alpha EMITTERS AND BLOBS DISCOVERED BY WISE: FEEDBACK CAUGHT IN THE ACT? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: formation; galaxies: high-redshift; galaxies: ISM; galaxies: starburst; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; SUBMILLIMETER-SELECTED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; AROMATIC-HYDROCARBON EMISSION; LUMINOUS INFRARED GALAXIES; DRIVEN STAR-FORMATION; QUASI-STELLAR OBJECT; GOODS SOUTH FIELD; BROAD-BAND SURVEY; EQUAL-TO 2.3 AB By combining data from the NASA Wide-field Infrared Survey Explorer (WISE) mission with optical spectroscopy from the W. M. Keck telescope, we discover a mid-IR color criterion that yields a 78% success rate in identifying rare, typically radio-quiet, 1.6 less than or similar to z less than or similar to 4.6 dusty Ly alpha emitters (LAEs). Of these, at least 37% have emission extended on scales of 30-100 kpc and are considered Ly alpha "blobs" (LABs). The objects have a surface density of only similar to 0.1 deg(-2), making them rare enough that they have been largely missed in deep, small area surveys. We measured spectroscopic redshifts for 92 of these galaxies, and find that the LAEs (LABs) have a median redshift of 2.3 (2.5). The WISE photometry coupled with data from Herschel (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) reveals that these galaxies are in the Hyper Luminous IR galaxy regime (L-IR greater than or similar to 10(13)-10(14) L-circle dot) and have warm colors. They are typically more luminous and warmer than other dusty, z similar to 2 populations such as submillimeter-selected galaxies and dust-obscured galaxies. These traits are commonly associated with the dust being illuminated by intense active galactic nucleus activity. We hypothesize that the combination of spatially extended Ly alpha, large amounts of warm IR-luminous dust, and rarity (implying a short-lived phase) can be explained if the galaxies are undergoing brief, intense "feedback" transforming them from an extreme dusty starburst/QSO into a mature galaxy. C1 [Bridge, Carrie R.] CALTECH, Pasadena, CA 91125 USA. [Blain, Andrew] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Borys, Colin J. K.; Griffith, Roger L.; Tsai, Chao-Wei] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Petty, Sara; Farrah, Duncan] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Benford, Dominic] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eisenhardt, Peter; Stern, Daniel; Wu, Jingwen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jarrett, Tom] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Lonsdale, Carol] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Wright, Edward L.; Wu, Jingwen] Univ Calif Los Angeles, Dept Astron, Los Angeles, CA 90095 USA. RP Bridge, CR (reprint author), CALTECH, MS249-17, Pasadena, CA 91125 USA. EM bridge@astro.caltech.edu RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU National Aeronautics and Space Administration; W. M. Keck Foundation FX The authors would like to thank the anonymous referee for suggestions that improved the clarity of this paper. This publication makes use of data products from the Wide-field Infrared Survey Explorer, a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 78 TC 36 Z9 36 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 JUN 1 PY 2013 VL 769 IS 2 AR UNSP 91 DI 10.1088/0004-637X/769/2/91 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100007 ER PT J AU Degenaar, N Miller, JM Kennea, J Gehrels, N Reynolds, T Wijnands, R AF Degenaar, N. Miller, J. M. Kennea, J. Gehrels, N. Reynolds, T. Wijnands, R. TI THE X-RAY FLARING PROPERTIES OF Sgr A* DURING SIX YEARS OF MONITORING WITH SWIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy: center; X-rays: individual (Sgr A*) ID SUPERMASSIVE BLACK-HOLE; CENTER CLOUD G2; ACTIVE GALACTIC NUCLEI; SOFT GAMMA-RAY; SAGITTARIUS-A; XMM-NEWTON; ELECTRON ACCELERATION; CHANDRA OBSERVATIONS; BRIGHTEST FLARE; STELLAR ORBITS AB Starting in 2006, Swift has been targeting a region of similar or equal to 21' x 21' around Sagittarius A* (Sgr A*) with the onboard X-Ray Telescope. The short, quasi-daily observations offer a unique view of the long-term X-ray behavior of the supermassive black hole. We report on the data obtained between 2006 February and 2011 October, which encompasses 715 observations with a total accumulated exposure time of similar or equal to 0.8 Ms. A total of six X-ray flares were detected with Swift, which all had an average 2-10 keV luminosity of L-X similar or equal to (1 - 3) x 10(35) erg s(-1) (assuming a distance of 8 kpc). This more than doubles the number of such bright X-ray flares observed from Sgr A*. One of the Swift-detected flares may have been softer than the other five, which would indicate that flares of similar intensity can have different spectral properties. The Swift campaign allows us to constrain the occurrence rate of bright (L-X greater than or similar to 10(35) erg s(-1)) X-ray flares to be similar or equal to 0.1-0.2 day(-1), which is in line with previous estimates. This analysis of the occurrence rate and properties of the X-ray flares seen with Swift offers an important calibration point to assess whether the flaring behavior of Sgr A* changes as a result of its interaction with the gas cloud that is projected to make a close passage in 2013. C1 [Degenaar, N.; Miller, J. M.; Reynolds, T.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Kennea, J.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. RP Degenaar, N (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM degenaar@umich.edu FU NASA from the Space Telescope Science Institute [HST-HF-51287.01-A]; NASA [NAS5-26555]; European Research Council; Penn State University by NASA [NAS5-00136] FX N.D. is supported by NASA through Hubble Postdoctoral Fellowship grant No. HST-HF-51287.01-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. R. W. is supported by a European Research Council starting grant. This work made use of public data from the Swift data archive, and data supplied by the UK Swift Science Data Center at the University of Leicester. Swift is supported at Penn State University by NASA Contract NAS5-00136. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. NR 65 TC 24 Z9 24 U1 1 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 JUN 1 PY 2013 VL 769 IS 2 AR UNSP 155 DI 10.1088/0004-637X/769/2/155 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100071 ER PT J AU Henry, A Martin, CL Finlator, K Dressler, A AF Henry, Alaina Martin, Crystal L. Finlator, Kristian Dressler, Alan TI THE METALLICITY EVOLUTION OF LOW-MASS GALAXIES: NEW CONSTRAINTS AT INTERMEDIATE REDSHIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: evolution ID STAR-FORMING GALAXIES; EMISSION-LINE GALAXIES; DIGITAL SKY SURVEY; SUBARU DEEP FIELD; H-II REGIONS; STELLAR MASS; LUMINOSITY FUNCTION; GALACTIC OUTFLOWS; COSMOLOGICAL SIMULATIONS; POPULATION SYNTHESIS AB We present abundance measurements from 26 emission-line-selected galaxies at z similar to 0.6-0.7. By reaching stellar masses as low as 10(8)M(circle dot), these observations provide the first measurement of the intermediate-redshift mass-metallicity (MZ) relation below 10(9)M(circle dot). For the portion of our sample above M > 10(9)M(circle dot) (8/26 galaxies), we find good agreement with previous measurements of the intermediate-redshift MZ relation. Compared to the local relation, we measure an evolution that corresponds to a 0.12 dex decrease in oxygen abundances at intermediate redshifts. This result confirms the trend that metallicity evolution becomes more significant toward lower stellar masses, in keeping with a downsizing scenario where low-mass galaxies evolve onto the local MZ relation at later cosmic times. We show that these galaxies follow the local fundamental metallicity relation, where objects with higher specific (mass-normalized) star formation rates (SFRs) have lower metallicities. Furthermore, we show that the galaxies in our sample lie on an extrapolation of the SFR-M-* relation (the star-forming main sequence). Leveraging the MZ relation and star-forming main sequence (and combining our data with higher-mass measurements from the literature), we test models that assume an equilibrium between mass inflow, outflow, and star formation. We find that outflows are required to describe the data. By comparing different outflow prescriptions, we show that momentum, driven winds can describe the MZ relation; however, this model underpredicts the amount of star formation in low-mass galaxies. This disagreement may indicate that preventive feedback from gas heating has been overestimated, or it may signify a more fundamental deviation from the equilibrium assumption. C1 [Henry, Alaina; Martin, Crystal L.; Finlator, Kristian] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Henry, Alaina] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Dressler, Alan] Carnegie Observ, Pasadena, CA 91101 USA. RP Henry, A (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM alaina.henry@nasa.gov RI Finlator, Kristian/M-4809-2014 OI Finlator, Kristian/0000-0002-0496-1656 FU W. M. Keck Foundation; National Aeronautics and Space Administration; NSF [AST-0808161, AST-1109288] FX Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.; The authors thank Jane Rigby, Dawn Erb, Joey Wong, Amber Straughn, Evan Skillman, Molly Peeples, Nicolas Bouche, Brian Siana, and Susan Kassin for insightful discussions. We also wish to thank the anonymous referee for helping to improve this manuscript. We are grateful to Esther Hu and Jabran Zahid for providing tabular data, and Peter Capak and the COSMOS team for the high-level science products that made this project possible. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work was supported by NSF grants AST-0808161 and AST-1109288. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 108 TC 31 Z9 31 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2013 VL 769 IS 2 AR UNSP 148 DI 10.1088/0004-637X/769/2/148 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100064 ER PT J AU Ireland, J Tolbert, AK Schwartz, RA Holman, GD Dennis, BR AF Ireland, J. Tolbert, A. K. Schwartz, R. A. Holman, G. D. Dennis, B. R. TI ESTIMATING THE PROPERTIES OF HARD X-RAY SOLAR FLARES BY CONSTRAINING MODEL PARAMETERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; Sun: flares; Sun: X-rays, gamma rays ID ELECTRON FLUX SPECTRA; NONUNIFORM IONIZATION; ENERGY PARTITION; ATOMIC DATABASE; EMISSION-LINES; ACCELERATION; RHESSI; DISTRIBUTIONS; SPECTROMETER; EXPLANATION AB We wish to better constrain the properties of solar flares by exploring how parameterized models of solar flares interact with uncertainty estimation methods. We compare four different methods of calculating uncertainty estimates in fitting parameterized models to Ramaty High Energy Solar Spectroscopic Imager X-ray spectra, considering only statistical sources of error. Three of the four methods are based on estimating the scale-size of the minimum in a hypersurface formed by the weighted sum of the squares of the differences between the model fit and the data as a function of the fit parameters, and are implemented as commonly practiced. The fourth method is also based on the difference between the data and the model, but instead uses Bayesian data analysis and Markov chain Monte Carlo (MCMC) techniques to calculate an uncertainty estimate. Two flare spectra are modeled: one from the Geostationary Operational Environmental Satellite X1.3 class flare of 2005 January 19, and the other from the X4.8 flare of 2002 July 23. We find that the four methods give approximately the same uncertainty estimates for the 2005 January 19 spectral fit parameters, but lead to very different uncertainty estimates for the 2002 July 23 spectral fit. This is because each method implements different analyses of the hypersurface, yielding method-dependent results that can differ greatly depending on the shape of the hypersurface. The hypersurface arising from the 2005 January 19 analysis is consistent with a normal distribution; therefore, the assumptions behind the three non-Bayesian uncertainty estimation methods are satisfied and similar estimates are found. The 2002 July 23 analysis shows that the hypersurface is not consistent with a normal distribution, indicating that the assumptions behind the three non-Bayesian uncertainty estimation methods are not satisfied, leading to differing estimates of the uncertainty. We find that the shape of the hypersurface is crucial in understanding the output from each uncertainty estimation technique, and that a crucial factor determining the shape of hypersurface is the location of the low-energy cutoff relative to energies where the thermal emission dominates. The Bayesian/MCMC approach also allows us to provide detailed information on probable values of the low-energy cutoff, E-c, a crucial parameter in defining the energy content of the flare-accelerated electrons. We show that for the 2002 July 23 flare data, there is a 95% probability that E-c lies below approximately 40 keV, and a 68% probability that it lies in the range 7-36 keV. Further, the low-energy cutoff is more likely to be in the range 25-35 keV than in any other 10 keV wide energy range. The low-energy cutoff for the 2005 January 19 flare is more tightly constrained to 107 +/- 4 keV with 68% probability. Using the Bayesian/ MCMC approach, we also estimate for the first time probability density functions for the total number of flare-accelerated electrons and the energy they carry for each flare studied. For the 2002 July 23 event, these probability density functions are asymmetric with long tails orders of magnitude higher than the most probable value, caused by the poorly constrained value of the low-energy cutoff. The most probable electron power is estimated at 10(28.1) erg s(-1), with a 68% credible interval estimated at 10(28.1)-10(29.0) erg s(-1), and a 95% credible interval estimated at 10(28.0)-10(30.2) erg s(-1). For the 2005 January 19 flare spectrum, the probability density functions for the total number of flare-accelerated electrons and their energy are much more symmetric and narrow: the most probable electron power is estimated at 10(27.66+/-0.01) erg s(-1) (68% credible intervals). However, in this case the uncertainty due to systematic sources of error is estimated to dominate the uncertainty due to statistical sources of error. C1 [Ireland, J.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA. [Tolbert, A. K.; Schwartz, R. A.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Holman, G. D.; Dennis, B. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ireland, J (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA. FU NASA ROSES award [NNH09ZDA001N-SHP]; HESPE (High Energy Solar Physics Data in Europe) collaboration FX This work was supported by a NASA ROSES award made under the opportunity NNH09ZDA001N-SHP entitled "Investigation of the low energy cutoff in solar flares," and by the HESPE (High Energy Solar Physics Data in Europe) collaboration. We are grateful to D. van Dyk and C. A. Young for their helpful suggestions. CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of Astrophysical Plasmas. It is a collaborative project involving the Naval Research Laboratory (USA), the University of Florence (Italy), the University of Cambridge, and the Rutherford Appleton Laboratory (UK). NR 40 TC 12 Z9 12 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2013 VL 769 IS 2 AR 89 DI 10.1088/0004-637X/769/2/89 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100005 ER PT J AU Moore, RL Sterling, AC Falconer, DA Robe, D AF Moore, Ronald L. Sterling, Alphonse C. Falconer, David A. Robe, Dominic TI THE COOL COMPONENT AND THE DICHOTOMY, LATERAL EXPANSION, AND AXIAL ROTATION OF SOLAR X-RAY JETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: activity; Sun: chromosphere; Sun: corona; Sun: magnetic topology ID HORIZONTAL MAGNETIC-FIELDS; QUIET-SUN INTERNETWORK; POLAR CORONAL HOLES; EXTREME-ULTRAVIOLET; BRIGHT POINTS; ENERGY-FLOW; HINODE; TELESCOPE; SPICULES; REGIONS AB We present results from a study of 54 polar X-ray jets that were observed in coronal X-ray movies from the X-ray Telescope on Hinode and had simultaneous coverage in movies of the cooler transition region (T similar to 10(5) K) taken in the He II 304 angstrom band of the Atmospheric Imaging Assembly (AIA) on Solar Dynamics Observatory. These dual observations verify the standard-jet/blowout-jet dichotomy of polar X-ray jets previously found primarily from XRT movies alone. In accord with models of blowout jets and standard jets, the AIA 304 angstrom movies show a cool (T similar to 10(5) K) component in nearly all blowout X-ray jets and in a small minority of standard X-ray jets, obvious lateral expansion in blowout X-ray jets but none in standard X-ray jets, and obvious axial rotation in both blowout X-ray jets and standard X-ray jets. In our sample, the number of turns of axial rotation in the cool-component standard X-ray jets is typical of that in the blowout X-ray jets, suggesting that the closed bipolar magnetic field in the jet base has substantial twist not only in all blowout X-ray jets but also in many standard X-ray jets. We point out that our results for the dichotomy, lateral expansion, and axial rotation of X-ray jets add credence to published speculation that type-II spicules are miniature analogs of X-ray jets, are generated by granule-size emerging bipoles, and thereby carry enough energy to power the corona and solar wind. C1 [Moore, Ronald L.; Sterling, Alphonse C.; Falconer, David A.] Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, Huntsville, AL 35812 USA. [Falconer, David A.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Falconer, David A.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Robe, Dominic] Tennessee Technol Univ, Dept Phys, Cookeville, TN 38505 USA. RP Moore, RL (reprint author), Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA. EM ron.moore@nasa.gov FU Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program; Hinode Project; NSF FX We thank the referee for insightful comments and suggestions that improved the paper. This work was funded by the Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program and the Hinode Project, and by the NSF through its Research Experience for Undergraduates Program. NR 50 TC 31 Z9 32 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 JUN 1 PY 2013 VL 769 IS 2 AR UNSP 134 DI 10.1088/0004-637X/769/2/134 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100050 ER PT J AU Schnittman, JD Krolik, JH Noble, SC AF Schnittman, Jeremy D. Krolik, Julian H. Noble, Scott C. TI X-RAY SPECTRA FROM MAGNETOHYDRODYNAMIC SIMULATIONS OF ACCRETING BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID QUASI-PERIODIC OSCILLATION; ACTIVE GALACTIC NUCLEI; XMM-NEWTON/EPIC-PN; LOW-HARD STATE; SEYFERT-GALAXIES; DOMINATED ACCRETION; LIGHT CURVES; CYGNUS X-1; TURBULENT COMPTONIZATION; ENERGY EXTRACTION AB We present the results of a new global radiation transport code coupled to a general relativistic magnetohydrodynamic simulation of an accreting, non-rotating black hole. For the first time, we are able to explain from first principles in a self-consistent way all the components seen in the X-ray spectra of stellar-mass black holes, including a thermal peak and all the features associated with strong hard X-ray emission: a power law extending to high energies, a Compton reflection hump, and a broad iron line. Varying only the mass accretion rate, we are able to reproduce a wide range of X-ray states seen in most galactic black hole sources. The temperature in the corona is T-e similar to 10 keV in a boundary layer near the disk and rises smoothly to T-e greater than or similar to 100 keV in low-density regions far above the disk. Even as the disk's reflection edge varies from the horizon out to approximate to 6M as the accretion rate decreases, we find that the shape of the Fe K alpha line is remarkably constant. This is because photons emitted from the plunging region are strongly beamed into the horizon and never reach the observer. We have also carried out a basic timing analysis of the spectra and find that the fractional variability increases with photon energy and viewer inclination angle, consistent with the coronal hot spot model for X-ray fluctuations. C1 [Schnittman, Jeremy D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krolik, Julian H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Noble, Scott C.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA. RP Schnittman, JD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jeremy.schnittman@nasa.gov; jhk@pha.jhu.edu; scn@astro.rit.edu FU NSF [AST-0507455, AST-0908336, AST-1028087]; National Science Foundation FX We thank C. Done, A. Fabian, T. Kallman, and C. Reynolds for helpful discussions. This work was partially supported by NSF grants AST-0507455 and AST-0908336 (J.H.K.) and AST-1028087 (S.C.N.). The ThinHR simulation was carried out on the Teragrid Ranger system at the Texas Advance Computing Center, which is supported in part by the National Science Foundation. NR 107 TC 31 Z9 31 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2013 VL 769 IS 2 AR UNSP 156 DI 10.1088/0004-637X/769/2/156 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100072 ER PT J AU Mangel, M MacCall, AD Brodziak, J Dick, EJ Forrest, RE Pourzand, R Ralston, S AF Mangel, Marc MacCall, Alec D. Brodziak, Jon Dick, E. J. Forrest, Robyn E. Pourzand, Roxanna Ralston, Stephen TI A perspective on steepness, reference points, and stock assessment SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID NEW-ENGLAND GROUNDFISH; WEST-COAST; FISHERIES MANAGEMENT; RECRUITMENT RELATIONSHIP; NATURAL MORTALITY; ASSESSMENT MODELS; HARVEST RATES; LIFE-HISTORY; PARAMETERS; SELECTIVITY AB We provide a perspective on steepness, reference points for fishery management, and stock assessment. We first review published data and give new results showing that key reference points are fixed when steepness and other life history parameters are fixed in stock assessments using a Beverton-Holt stock-recruitment relationship. We use both production and age-structured models to explore these patterns. For the production model, we derive explicit relationships for steepness and life history parameters and then for steepness and major reference points. For the age-structured model, we are required to generally use numerical computation, and so we provide an example that complements the analytical results of the production model. We discuss what it means to set steepness equal to 1 and how to construct a prior for steepness. Ways out of the difficult situation raised by fixing steepness and life history parameters include not fixing them, using a more complicated stock-recruitment relationship, and being more explicit about the information content of the data and what that means for policy makers. We discuss the strengths and limitations of each approach. C1 [Mangel, Marc; Pourzand, Roxanna] Univ Calif Santa Cruz, Ctr Stock Assessment Res, Santa Cruz, CA 95064 USA. [Mangel, Marc] Univ Bergen, Dept Biol, N-5020 Bergen, Norway. [MacCall, Alec D.; Dick, E. J.; Ralston, Stephen] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Santa Cruz, CA 95060 USA. [Brodziak, Jon] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. [Forrest, Robyn E.] Fisheries & Oceans Canada, Pacific Biol Stn, Nanaimo, BC V9T 6N7, Canada. RP Mangel, M (reprint author), Univ Calif Santa Cruz, Ctr Stock Assessment Res, MS E-2, Santa Cruz, CA 95064 USA. EM msmangel@soe.ucsc.edu FU Pacific Islands Fisheries Science Center; Center for Stock Assessment Research; Southwest Fisheries Science Center Santa Cruz Laboratory; University of California Santa Cruz FX This work was supported by the Pacific Islands Fisheries Science Center through a contract to Marine Resources Assessment Group (MRAG) Americas and by the Center for Stock Assessment Research, a partnership between the Southwest Fisheries Science Center Santa Cruz Laboratory and the University of California Santa Cruz. We thank reviewers (the Associate Editor, one anonymous reviewer, Chris Francis, and Michael Sissenwine), colleagues at the Northwest Fisheries Science Center, and Ian Boyd, Bill de la Mare, and Sidney Holt for thoughtful comments that lead us to new insights and in new directions. NR 78 TC 19 Z9 19 U1 3 U2 48 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD JUN PY 2013 VL 70 IS 6 BP 930 EP 940 DI 10.1139/cjfas-2012-0372 PG 11 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 160FC UT WOS:000320101500013 ER PT J AU Hipkin, VJ Voytek, MA Meyer, MA Leveille, R Domagal-Goldman, SD AF Hipkin, V. J. Voytek, M. A. Meyer, M. A. Leveille, R. Domagal-Goldman, S. D. TI Analogue sites for Mars missions: NASA's Mars Science Laboratory and beyond - Overview of an international workshop held at The Woodlands, Texas, on March 5-6, 2011 SO ICARUS LA English DT Editorial Material ID METHANE AB Recent research results from analogue sites, with a strong focus on astrobiology-related investigations, are presented in this special issue on 'Analogue sites for Mars missions'. In addition, this article describes workshop discussions and a resulting improved framework for reporting, evaluating, and comparing analogue sites. Developed through consideration of a broad range of sites, including many of those described in this special issue, this framework comprises an analogue site abstract, a rubric for the scientific evaluation of analogue sites, and a rubric for logistical information. An overview of the Mars Analogues Workshop is provided, and the rubrics are presented for further discussion. Crown Copyright (c) 2013 Published by Elsevier Inc. All rights reserved. C1 [Hipkin, V. J.; Leveille, R.] Canadian Space Agcy, John H Chapman Space Ctr, St Hubert, PQ J3Y 8Y9, Canada. [Voytek, M. A.; Meyer, M. A.] NASA Headquarters, Washington, DC 20546 USA. [Domagal-Goldman, S. D.] UW Astron, Seattle, WA 98195 USA. RP Hipkin, VJ (reprint author), Canadian Space Agcy, John H Chapman Space Ctr, 6767 Route Aeroport, St Hubert, PQ J3Y 8Y9, Canada. EM victoria.hipkin@asc-csa.gc.ca RI Domagal-Goldman, Shawn/F-3521-2012 OI Domagal-Goldman, Shawn/0000-0003-0354-9325 NR 21 TC 1 Z9 1 U1 1 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JUN PY 2013 VL 224 IS 2 SI SI BP 261 EP 267 DI 10.1016/j.icarus.2013.02.021 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200001 ER PT J AU Tazaz, AM Bebout, BM Kelley, CA Poole, J Chanton, JP AF Tazaz, Amanda M. Bebout, Brad M. Kelley, Cheryl A. Poole, Jennifer Chanton, Jeffrey P. TI Redefining the isotopic boundaries of biogenic methane: Methane from endoevaporites SO ICARUS LA English DT Article DE Astrobiology; Mars; Organic chemistry ID SULFATE-REDUCING BACTERIA; HYPERSALINE MICROBIAL MAT; BAJA-CALIFORNIA-SUR; GUERRERO-NEGRO; HYDROCARBON GASES; METHYLATED AMINES; LAGUNA MORMONA; MEXICO; SEDIMENTS; MARS AB The recent reports of methane in the atmosphere of Mars, as well as the findings of hypersaline paleoenvironments on that planet, have underscored the need to evaluate the importance of biological (as opposed to geological) trace gas production and consumption, particularly in hypersaline environments. Methane in the atmosphere of Mars may be an indication of extant life, but it may also be a consequence of geologic activity and/or the thermal alteration of ancient organic matter. On Earth these methane sources can be distinguished using stable isotopic analyses and the ratio of methane (C-1) to C-2 and C-3 alkanes present in the gas source (C-1/(C-2 + C-3)). We report here that methane produced in hypersaline environments on Earth has an isotopic composition and alkane content outside the values presently considered to indicate a biogenic origin. Methane-rich bubbles released from sub-aqueous substrates contained delta C-13(CH4) and delta H-2(CH4) values ranging from -65 parts per thousand to -35 parts per thousand and -350 parts per thousand to -140 parts per thousand respectively. Higher salinity endoevaporites yielded what would be considered non-biogenic methane based upon stable isotopic and alkane content, however incubation of crustal and algal mat samples resulted in methane production with similar isotopic values. Radiocarbon analysis indicated that the production of the methane was from recently fixed carbon. An extension of the isotopic boundaries of biogenic methane is necessary in order to avoid the possibility of false negatives returned from measurements of methane on Mars and other planetary bodies. Published by Elsevier Inc. C1 [Tazaz, Amanda M.; Chanton, Jeffrey P.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Bebout, Brad M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Kelley, Cheryl A.; Poole, Jennifer] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. RP Bebout, BM (reprint author), NASA, Ames Res Ctr, Exobiol Branch, MS 239-4, Moffett Field, CA 94035 USA. EM Brad.M.Bebout@nasa.gov RI Kelley, Cheryl/K-9392-2015 FU NASA's Exobiology Program; Florida State University; University of Missouri; Florida Education Fund McKnight Fellowship FX We thank Exportadora de Sal, S.A. de C.V., US Fish and Wildlife Service, and Don Edwards National Wildlife Refuge for access to their salt ponds. We thank Angela Detweiler, Adrienne Frisbee and Claire Langford for excellent technical support in the laboratory and in the field. This research was supported by NASA's Exobiology Program, Florida State University and the University of Missouri. A.M.T. was supported by the Florida Education Fund McKnight Fellowship. NR 64 TC 11 Z9 11 U1 0 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2013 VL 224 IS 2 SI SI BP 268 EP 275 DI 10.1016/j.icarus.2012.06.008 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200002 ER PT J AU Etiope, G Ehlmann, BL Schoell, M AF Etiope, Giuseppe Ehlmann, Bethany L. Schoell, Martin TI Low temperature production and exhalation of methane from serpentinized rocks on Earth: A potential analog for methane production on Mars SO ICARUS LA English DT Article DE Mars; Earth; Geological processes; Mineralogy ID HYDROGEN ISOTOPE FRACTIONATION; MARTIAN ATMOSPHERE; ZAMBALES OPHIOLITE; SAMAIL OPHIOLITE; CARBON-DIOXIDE; GROUND ICE; GAS SEEPS; WATER; ORIGIN; FRACTURE AB We evaluate, based on terrestrial analogs, the potential flux, origin and isotopic signature of methane (CH4) from serpentinized or serpentinizing rocks on Mars. The Tekirova ophiolites, in Turkey, have been shown to release, either via focused vents or through diffuse microseepage, substantial amounts of CH4 which could be produced via catalyzed abiotic methanation (Sabatier reaction) at low temperatures (<50 degrees C). Serpentinized ultramafic rocks on Mars are likely to have necessary chemical constituents for methane production and fractures for release of gas to the atmosphere, similar to those on Earth. A simple, first-order estimation gas-advection model suggests that methane fluxes on the order of several mg m(-2) d(-1), similar to microseepage observed in terrestrial ophiolites, could occur in martian rocks. High temperature, hydrothermal conditions may not be necessary for abiotic CH4 synthesis on Mars: low temperature (<50 degrees C) methanation is possible in the presence of catalysts like ruthenium, rhodium or, more commonly, chromium minerals, which occur in terrestrial ophiolites as in martian mantle meteorites. The terrestrial analog environment of abiotic microseepage may thus explain production of methane on Mars in the ancient past or at present. The wide range of martian C-12/C-13 and D/H ratios and the potential secondary alteration of CH4 by abiotic oxidation, as observed on Earth, could result in large isotope variations of methane on Mars. CH4 isotopic composition alone may not allow definitive determination of biotic vs. abiotic gas origin. Using our terrestrial vs. martian analysis as guide to future Mars exploration we propose that direct methane and ethane gas detection and isotopic measurements on the ground over serpentinized/serpentinizing rocks should be considered in developing future strategies for unraveling the source and origin of methane on Mars. (c) 2012 Elsevier Inc. All rights reserved. C1 [Etiope, Giuseppe] Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. [Etiope, Giuseppe] Univ Babes Bolyai, Fac Environm Sci & Engn, Cluj Napoca 400294, Romania. [Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schoell, Martin] GasConsult Int Inc, Berkeley, CA 94703 USA. RP Etiope, G (reprint author), Ist Nazl Geofis & Vulcanol, Sez Roma 2,Via V Murata 605, I-00143 Rome, Italy. EM etiope@ingv.it RI Etiope, Giuseppe/H-3343-2011 OI Etiope, Giuseppe/0000-0001-8614-4221 FU Research and Scientific Support Department of the European Space Agency (ESA-RSSD) FX This work is part of the "Interdisciplinary Study of Methane on Mars" funded by the Research and Scientific Support Department of the European Space Agency (ESA-RSSD) and coordinated by Olivier Witasse. Ravindranathan Thampi provided useful inputs about catalyzed methanation. Thanks are due to three anonymous reviewers for their valuable comments and suggestions to improve the paper. NR 84 TC 19 Z9 19 U1 4 U2 41 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2013 VL 224 IS 2 SI SI BP 276 EP 285 DI 10.1016/j.icarus.2012.05.009 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200003 ER PT J AU Stern, JC McAdam, AC Ten Kate, IL Bish, DL Blake, DF Morris, RV Bowden, R Fogel, ML Glamoclija, M Mahaffy, PR Steele, A Amundsen, HEF AF Stern, Jennifer C. McAdam, Amy C. Ten Kate, Inge L. Bish, David L. Blake, David F. Morris, Richard V. Bowden, Roxane Fogel, Marilyn L. Glamoclija, Mihaela Mahaffy, Paul R. Steele, Andrew Amundsen, Hans E. F. TI Isotopic and geochemical investigation of two distinct Mars analog environments using evolved gas techniques in Svalbard, Norway SO ICARUS LA English DT Article ID PHOENIX LANDING SITE; MARTIAN METEORITE ALH84001; EXOBIOLOGICAL IMPLICATIONS; JANUSFJELLET SUBGROUP; WEATHERING PRODUCTS; CARBONATE GLOBULES; TERRESTRIAL ANALOG; HYDROCARBON SEEPS; ORGANIC-COMPOUNDS; ICE INTERACTIONS AB The 2010 Arctic Mars Analog Svalbard Expedition (AMASE) investigated two distinct geologic settings on Svalbard, using methodologies and techniques to be deployed on Mars Science Laboratory (MSL). AMASE-related research comprises both analyses conducted during the expedition and further analyses of collected samples using laboratory facilities at a variety of institutions. The Sample Analysis at Mars (SAM) instrument suite on MSL includes pyrolysis ovens, a gas-processing manifold, a quadrupole mass spectrometer (QMS), several gas chromatography columns, and a Tunable Laser Spectrometer (TLS). An integral part of SAM development is the deployment of SAM-like instrumentation in the field. During AMASE 2010, two parts of SAM participated as stand-alone instruments. A Hiden Evolved Gas Analysis-Mass Spectrometer (EGA-QMS) system represented the EGA-QMS component of SAM, and a Picarro Cavity Ring Down Spectrometer (EGA-CRDS), represented the EGA-TLS component of SAM. A field analog of CheMin, the XRD/XRF on MSL, was also deployed as part of this field campaign. Carbon isotopic measurements of CO2 evolved during thermal decomposition of carbonates were used together with EGA-QMS geochemical data, mineral composition information and contextual observations made during sample collection to distinguish carbonates formation associated with chemosynthetic activity at a fossil methane seep from abiotic processes forming carbonates associated with subglacial basaltic eruptions. Carbon and oxygen isotopes of the basalt-hosted carbonates suggest cryogenic carbonate formation, though more research is necessary to clarify the history of these rocks. Published by Elsevier Inc. C1 [Stern, Jennifer C.; McAdam, Amy C.; Ten Kate, Inge L.; Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20910 USA. [Ten Kate, Inge L.] Univ Oslo, Ctr Phys Geol Proc, N-0316 Oslo, Norway. [Bish, David L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Blake, David F.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, Astromat Branch, Houston, TX 77058 USA. [Bowden, Roxane; Fogel, Marilyn L.; Glamoclija, Mihaela; Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Amundsen, Hans E. F.] Earth & Planetary Explorat Serv, Oslo, Norway. RP Stern, JC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Code 699, Greenbelt, MD 20910 USA. EM Jennifer.C.Stern@nasa.gov RI Stern, Jennifer/E-3135-2012; Fogel, Marilyn/M-2395-2015 OI Stern, Jennifer/0000-0002-0162-8807; Fogel, Marilyn/0000-0002-1176-3818 FU NASA's Astrobiology Science and Technology for Exploring Planets (ASTEP) Program FX The authors would like to acknowledge NASA's Astrobiology Science and Technology for Exploring Planets (ASTEP) Program for funding, the entire 2010 AMASE Team, the Ny Alesund community, the Norwegian Polar Institute, and the European Space Agency. The authors also thank two anonymous reviewers for their helpful comments. NR 92 TC 4 Z9 4 U1 5 U2 32 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 JUN PY 2013 VL 224 IS 2 SI SI BP 297 EP 308 DI 10.1016/j.icarus.2012.07.010 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200005 ER PT J AU Bishop, JL Franz, HB Goetz, W Blake, DF Freissinet, C Steininger, H Goesmann, F Brinckerhoff, WB Getty, S Pinnick, VT Mahaffy, PR Dyar, MD AF Bishop, Janice L. Franz, Heather B. Goetz, Walter Blake, David F. Freissinet, Caroline Steininger, Harald Goesmann, Fred Brinckerhoff, William B. Getty, Stephanie Pinnick, Veronica T. Mahaffy, Paul R. Dyar, M. Darby TI Coordinated analyses of Antarctic sediments as Mars analog materials using reflectance spectroscopy and current flight-like instruments for CheMin, SAM and MOMA SO ICARUS LA English DT Article DE Mars; surface; Mineralogy; Organic chemistry; Spectroscopy ID MCMURDO DRY VALLEYS; INDUCED BREAKDOWN SPECTROSCOPY; MARTIAN METEORITE ALH84001; COVERED LAKE-HOARE; RAMAN-SPECTROSCOPY; IN-SITU; GEOCHEMICAL ANALYSES; TAYLOR VALLEY; ICE; MINERALS AB Coordinated analyses of mineralogy and chemistry of sediments from the Antarctic Dry Valleys illustrate how data obtained using flight-ready technology of current NASA and ESA missions can be combined for greater understanding of the samples. Mineralogy was measured by X-ray diffraction (XRD) and visible/near-infrared (VNIR) reflectance spectroscopy. Chemical analyses utilized a quadrupole mass spectrometer (QMS) to perform pyrolysis-evolved gas analysis (EGA) and gas chromatography-mass spectrometry (GC/MS) both with and without derivatization, as well as laser desorption-mass spectrometry (LD/MS) techniques. These analyses are designed to demonstrate some of the capabilities of near-term landed Mars missions, to provide ground truthing of VNIR reflectance data acquired from orbit by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on MRO and to provide detection limits for surface-operated instruments: the Chemistry and Mineralogy (CheMin) and Sample Analysis at Mars (SAM) instrument suites onboard Mars Science Laboratory (MSL) and the Mars Organic Molecule Analyzer (MOMA) onboard ExoMars-2018. The new data from this study are compared with previous analyses of the sediments performed with other techniques. Tremolite was found in the oxic region samples for the first time using the CheMin-like XRD instrument. The NIR spectral features of tremolite are consistent with those observed in these samples. Although the tremolite bands are weak in spectra of these samples, spectral features near 2.32 and 2.39 mu m could be detected by CRISM if tremolite is present on the martian surface. Allophane was found to be a good match to weak NIR features at similar to 1.37-1.41, 1.92, and 2.19 mu m in spectra of the oxic region sediments and is a common component of immature volcanic soils. Biogenic methane was found to be associated with calcite in the oxic region samples by the SAM/EGA instrument and a phosphoric acid derivative was found in the anoxic region sample using the SAM/MTBSTFA technique. (c) 2012 Elsevier Inc. All rights reserved. C1 [Bishop, Janice L.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Bishop, Janice L.; Blake, David F.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Franz, Heather B.; Freissinet, Caroline; Brinckerhoff, William B.; Getty, Stephanie; Pinnick, Veronica T.; Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA. [Franz, Heather B.; Freissinet, Caroline; Pinnick, Veronica T.] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Goetz, Walter; Steininger, Harald; Goesmann, Fred] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. RP Bishop, JL (reprint author), Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. EM jbishop@seti.org RI Getty, Stephanie/D-7037-2012; freissinet, caroline/F-2431-2012; Brinckerhoff, William/F-3453-2012; OI Brinckerhoff, William/0000-0001-5121-2634; Steininger, Harald/0000-0003-4880-1635 FU NSF's Office of Polar Programs; NASA's PGG program FX The authors are grateful to NSF's Office of Polar Programs for sponsoring collection of these samples from the Dry Valleys, to Dr. T. Hiroi for assistance measuring the reflectance spectra, and to Dr. J. Wray for helpful editorial comments. Thanks are also due to NASA's PGG program for supporting Brown University's RELAB facility. NR 94 TC 12 Z9 12 U1 6 U2 41 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2013 VL 224 IS 2 SI SI BP 309 EP 325 DI 10.1016/j.icarus.2012.05.014 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200006 ER PT J AU Wierzchos, J Davila, AF Artieda, O Camara-Gallego, B Rios, AD Nealson, KH Valea, S Garcia-Gonzalez, MT Ascaso, C AF Wierzchos, Jacek Davila, Alfonso F. Artieda, Octavio Camara-Gallego, Beatriz Rios, Asuncion de los Nealson, Kenneth H. Valea, Sergio Garcia-Gonzalez, M. Teresa Ascaso, Carmen TI Ignimbrite as a substrate for endolithic life in the hyper-arid Atacama Desert: Implications for the search for life on Mars SO ICARUS LA English DT Article DE Geophysics; Mars; Search for extraterrestrial life ID ARCTIC CRYPTOENDOLITHIC HABITATS; BIOWEATHERED GRANITIC BIOTITE; VOLCANIC GLASS; MICROBIAL LIFE; APOLLINARIS-PATERA; LICHEN ACTIVITY; MINERAL SOILS; COLONIZATION; CYANOBACTERIA; COMMUNITIES AB The hyper-arid core of the Atacama Desert in Chile is considered the driest and most life-limited place on Earth, with few habitats capable of sustaining an active microbial ecosystem. As such, it is one of the best terrestrial analogues of the extreme arid conditions on Mars, and an ideal environment to explore survival and biological adaptation strategies as the environment becomes increasingly dry. Here we show that weakly welded rhyolitic ignimbrites in this desert are abundantly colonized by endolithic cyanobacteria and associated heterotrophic bacteria. We propose that the porous ignimbrite interior provides protection from damaging UV radiation and excessive levels of visible light. Rock porosity also favors cell hydration through water retention after scarce rainfall events, even when the surrounding environment remains stubbornly dry. This is the first known example of an endolithic microbial community colonizing ignimbrite rocks in an extremely dry environment. The existence of a habitat capable of supporting abundant phototrophic and heterotrophic communities in an environment that precludes most life forms suggests that, if similar deposits are found on Mars, these should be considered important targets in the search for life. Indeed, ignimbrite rocks have been tentatively identified in Gale Crater, the landing site of the Mars Science Laboratory (MSL) mission and could be directly analyzed by its rover Curiosity. (c) 2012 Elsevier Inc. All rights reserved. C1 [Wierzchos, Jacek; Camara-Gallego, Beatriz; Rios, Asuncion de los; Valea, Sergio; Ascaso, Carmen] CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. [Davila, Alfonso F.] NASA, Ames Res Ctr, Moffett Field, CA 95136 USA. [Artieda, Octavio] Univ Extremadura, Plasencia 10600, Spain. [Nealson, Kenneth H.] Univ So Calif, Los Angeles, CA 90089 USA. [Garcia-Gonzalez, M. Teresa] CSIC, Inst Ciencias Agr, E-28006 Madrid, Spain. RP Wierzchos, J (reprint author), CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. EM j.wierzchos@mncn.csic.es RI de los Rios, Asuncion/L-3694-2014; Ascaso, Carmen/F-5369-2011; Camara Gallego, Beatriz/H-6407-2015 OI de los Rios, Asuncion/0000-0002-0266-3516; Ascaso, Carmen/0000-0001-9665-193X; Camara Gallego, Beatriz/0000-0003-4945-3134 FU Spanish Ministry of Science and Innovation [CGL2010-16004, CTM 2009-12838-C04-03]; NASA Exobiology program [NNX12AD61G] FX The authors thank F. Pinto, V. Souza-Egipsy and T. Carnota for technical assistance, and L. Tormo for help with the ESEM, R. Gonzalez with the FRX, M. Juanco with the XRD, and A.L. Duque and D. Gamarra with the MIP work. D. Herrera is thanked for field assistance in the Atacama Desert. We also thank A. Burton for polishing our English. This work was funded by grant CGL2010-16004 and CTM 2009-12838-C04-03 from the Spanish Ministry of Science and Innovation. A.F.D., O.A. and J.W. were supported by Grant NNX12AD61G of the NASA Exobiology program. NR 79 TC 16 Z9 16 U1 9 U2 67 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2013 VL 224 IS 2 SI SI BP 334 EP 346 DI 10.1016/j.icarus.2012.06.009 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200008 ER PT J AU Battler, MM Osinski, GR Lim, DSS Davila, AF Michel, FA Craig, MA Izawa, MRM Leoni, L Slater, GF Fairen, AG Preston, J Banerjee, NR AF Battler, Melissa M. Osinski, Gordon R. Lim, Darlene S. S. Davila, Alfonso F. Michel, Frederick A. Craig, Michael A. Izawa, Matthew R. M. Leoni, Lisa Slater, Gregory F. Fairen, Alberto G. Preston, Louisa J. Banerjee, Neil R. TI Characterization of the acidic cold seep emplaced jarositic Golden Deposit, NWT, Canada, as an analogue for jarosite deposition on Mars SO ICARUS LA English DT Article DE Mars; Geological processes; Mineralogy; Spectroscopy; Astrobiology ID SOLID-SOLUTION SERIES; MERIDIANI-PLANUM; RIO-TINTO; TERRESTRIAL ANALOGS; NORTHWEST-TERRITORIES; OPPORTUNITY ROVER; SULFATE MINERALS; SUBSURFACE WATER; SOUTHWEST SPAIN; LANDING SITE AB Surficial deposits of the OH-bearing iron sulfate mineral jarosite have been observed in several places on Mars, such as Meridiani Planum and Mawrth Vallis. The specific depositional conditions and mechanisms are not known, but by comparing martian sites to analogous locations on Earth, the conditions of formation and, thus, the martian depositional paleoenvironments may be postulated. Located in a cold semi-arid desert similar to 100 km east of Norman Wells, Northwest Territories, Canada, the Golden Deposit (GD) is visible from the air as a brilliant golden-yellow patch of unvegetated soil, approximately 140 m x 50 m. The GD is underlain by permafrost and consists of yellow sediment, which is precipitating from seeps of acidic, iron-bearing groundwater. On the surface, the GD appears as a patchwork of raised polygons, with acidic waters flowing from seeps in troughs between polygonal islands. Although UV-Vis-NIR spectral analysis detects only jarosite, mineralogy, as determined by X-ray diffraction and inductively coupled plasma emission spectrometry, is predominantly natrojarosite and jarosite, with hydronium jarosite, goethite, quartz, clays, and small amounts of hematite. Water pH varies significantly over short distances depending on proximity to acid seeps, from 2.3 directly above seeps, to 5.7 several m downstream from seeps within the deposit, and up to 6.5 in ponds proximal to the deposit. Visual observations of microbial filament communities and phospholipid fatty acid analyses confirm that the GD is capable of supporting life for at least part of the year. Jarosite-bearing sediments extend beneath vegetation up to 70 m out from the deposit and are mixed with plant debris and minerals presumably weathered from bedrock and glacial till. This site is of particular interest because mineralogy (natrojarosite, jarosite, hematite, and goethite) and environmental conditions (permafrost and arid conditions) at the time of deposition are conceivably analogous to jarosite deposits on Mars. Most terrestrial analogues for Mars jarosites have been identified in temperate environments, where evaporation rates are very high and jarosites form along with other sulfates due to rapid evaporation (e.g. Rio Tinto, Spain; Western Australian acidic saline lake deposits). The GD is a rare example of an analogue site where jarosite precipitates under dominant freezing processes similar to those which could have prevailed on early Mars. Thus, the GD offers a new perspective on jarosite deposition by the upwelling of acidic waters through permafrost at Meridiani Planum and Mawrth Vallis, Mars. The GD also demonstrates that martian deposits may show considerably more chemical and mineral variability than indicated by the current remote sensing data sets. (c) 2012 Elsevier Inc. All rights reserved. C1 [Battler, Melissa M.; Osinski, Gordon R.; Craig, Michael A.; Izawa, Matthew R. M.; Preston, Louisa J.; Banerjee, Neil R.] Univ Western Ontario, Ctr Planetaty Sci & Explorat, Dept Earth Sci, London, ON N6A 5B7, Canada. [Osinski, Gordon R.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 5B7, Canada. [Lim, Darlene S. S.; Davila, Alfonso F.; Fairen, Alberto G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lim, Darlene S. S.; Davila, Alfonso F.; Fairen, Alberto G.] SETI Inst, Mountain View, CA 94043 USA. [Michel, Frederick A.] Carleton Univ, Inst Environm Sci, Ottawa, ON K1S 5B6, Canada. [Leoni, Lisa; Slater, Gregory F.] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4K1, Canada. RP Battler, MM (reprint author), Univ Western Ontario, Ctr Planetaty Sci & Explorat, Dept Earth Sci, 1151 Richmond St, London, ON N6A 5B7, Canada. EM mbattle@uwo.ca RI Battler, Melissa/N-2591-2014; OI Izawa, Matthew/0000-0001-5456-2912 FU Canadian Space Agency (CSA) Canadian Analogue Research Network (CARN); Natural Science and Engineering Research Council of Canada (NSERC) FX Roberta Flemming is thanked for guidance with mineral identification and the use of the EVA software, and Kim Law is thanked for guidance with the use of the XRD. Nicola Barry is thanked for assistance in the lab. We also wish to thank two anonymous reviewers for their helpful feedback. This study was supported by grants from the Canadian Space Agency (CSA) Canadian Analogue Research Network (CARN) and the Natural Science and Engineering Research Council of Canada (NSERC) to GRO. NR 72 TC 5 Z9 5 U1 2 U2 29 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 JUN PY 2013 VL 224 IS 2 SI SI BP 382 EP 398 DI 10.1016/j.icarus.2012.05.015 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200011 ER PT J AU Clarke, JDA Stoker, CR AF Clarke, Jonathan D. A. Stoker, Carol R. TI Searching for stromatolites: The 3.4 Ga Strelley Pool Formation (Pilbara region, Western Australia) as a Mars analogue SO ICARUS LA English DT Article DE Astrobiology; Mars, surface; Search for extraterrestrial life ID NORTH-POLE; ARCHEAN STROMATOLITES; FOSSIL BACTERIA; EARLY-LIFE; CRATON; ENVIRONMENT; CHERT; GEOCHEMISTRY; MICROFOSSILS; BIOGENICITY AB Stromatolites are readily identified, outcrop scale indicators of potential biological activity, even though constructed by microbes. Their presence in -J.5 Ga volcano-sedimentary successions of the Pilbara region of Western Australia suggests that they might also occur in similar, Noachian-agc successions On Mars. Field and basic laboratory studies of one such occurrence near Nullagine highlight many issues that would be faced by any stromatolite search strategy on Mars. Firstly, the stromatolites are found in local aggregations that make up a very small part of the overall succession, possibly as little as one millionth of the outcrop area. An effective search strategy would require a combination of remote sensing to highlight features with high probability of hosting stromatolites, precision landing, and extensive cross-country mobility, difficult to achieve with a purely unmanned exploration system. Secondly, the limited analytical suite available to any unmanned mission would make conclusive determination of the biogenicity of any stromatolite-like feature on Mars very difficult. This is shown by the controversy over the biogenicity of the Pilbara examples, despite a much greater range of analytical techniques applied to the Pilbara examples. Once possible stromatolites features have been found on Mars, sample return would be imperative to determine their biogenicity. (c) 2013 Elsevier Inc. All rights reserved. C1 [Clarke, Jonathan D. A.] Mars Soc Australia, Monash, ACT 2904, Australia. [Stoker, Carol R.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Clarke, JDA (reprint author), Mars Soc Australia, C-O 43 Michell St, Monash, ACT 2904, Australia. EM Jon.Clarke@bigpond.com FU Royalties for Regions of the Western Australian Government; CSIRO; The Pilbara Development Commission; NASA Spaceward Bound; MSA FX Funding for the Spaceward Bound Pilbara Expedition was provided by Royalties for Regions of the Western Australian Government, CSIRO, The Pilbara Development Commission, NASA Spaceward Bound, MSA, and individual donors. The PIMA was loaned to the lead author by Liz Webber of Geoscience Australia. We thank Kath Grey, an anonymous reviewer and the editor of Icarus for their helpful comments in preparing this manuscript for publication. NR 53 TC 4 Z9 4 U1 6 U2 20 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JUN PY 2013 VL 224 IS 2 SI SI BP 413 EP 423 DI 10.1016/j.icarus.2013.02.006 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200013 ER PT J AU Allen, CC Oehler, DZ Etiope, G Van Rensbergen, P Baciu, C Feyzullayev, A Martinelli, G Tanaka, K Van Rooij, D AF Allen, Carlton C. Oehler, Dorothy Z. Etiope, Giuseppe Van Rensbergen, Pieter Baciu, Calin Feyzullayev, Akper Martinelli, Giovanni Tanaka, Kazuhiro Van Rooij, David TI Fluid expulsion in terrestrial sedimentary basins: A process providing potential analogs for giant polygons and mounds in the martian lowlands SO ICARUS LA English DT Article DE Mars; Mars, Surface; Geological processes; Earth ID LOWER CONGO BASIN; EASTERN MEDITERRANEAN SEA; FINE-GRAINED SEDIMENTS; MID-NORWEGIAN MARGIN; MUD VOLCANO FIELD; FAULT SYSTEMS; NORTH-SEA; SPATIAL-DISTRIBUTION; FLOOR POCKMARKS; UTOPIA PLANITIA AB On Earth, burial of fine-grained sediments in offshore passive margins (e.g., underwater fans and deltas) commonly results in fluid expulsion features including large-scale polygonal fractures, mud volcanoes, and pockmarks. Comparison of resulting offshore polygons and mud volcanoes with giant polygons and high-albedo mounds in the Chryse-Acidalia region of Mars shows the terrestrial and martian features to be similar in size, morphology, geologic context, and general co-occurrence within the same basin. These similarities suggest that the process of terrestrial fluid expulsion may provide an analog that could link the giant polygons and mounds in Chryse and Acidalia to a single process. Moreover, while the terrestrial offshore polygons and mud volcanoes commonly develop in the same basins, these features do not necessarily occur in exactly the same locations within those basins, as they are independent responses to compaction and dewatering. Thus, the fluid expulsion analog does not require that the martian giant polygons and mounds have identical distributions. This is the situation in Chryse and Acidalia where the giant polygons and mounds are extensively developed and generally have overlapping distributions, but where each set of features may occur in places without the other. This fluid expulsion analog is enhanced by the fact that giant polygons and mounds in Chryse and Acidalia co-occur in a regional sense and in a geologic setting that is consistent with a fluid expulsion model of formation. Implications of this analog may impact our view of the role of water in the depositional history of the martian lowlands. Published by Elsevier Inc. C1 [Allen, Carlton C.; Oehler, Dorothy Z.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. [Etiope, Giuseppe] Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. [Van Rensbergen, Pieter] Shell Int Explorat & Prod BV, NL-2288 GS Rijswijk, Netherlands. [Etiope, Giuseppe; Baciu, Calin] Univ Babes Bolyai, Fac Environm Sci & Engn, R-3400 Cluj Napoca, Romania. [Feyzullayev, Akper] Natl Acad Sci, Geol Inst Azerbaijan, Petr Geol & Geochem Dept, AZ-1143 Baku, Azerbaijan. [Martinelli, Giovanni] Agenzia Reg Prevenz & Ambiente Emilia Romagna, I-42100 Reggio Emilia, Italy. [Tanaka, Kazuhiro] Yamaguchi Univ, Grad Sch Sci & Engn, Dept Earth Sci, Yamaguchi, Japan. [Van Rooij, David] Univ Ghent, Renard Ctr Marine Geol, Dept Geol & Soil Sci, B-9000 Ghent, Belgium. RP Allen, CC (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, 2101 NASA Pkwy, Houston, TX 77058 USA. EM carlton.c.allen@nasa.gov; dorothy.z.oehler@nasa.gov; etiope@ingv.it; Pieter.VanRensbergen@shell.com; calin.baciu@ubbcluj.ro; fakper@gmail.com; Giovanni.martinelli15@tin.it; ka-tanak@yamaguchi-u.ac.jp; david.vanrooij@ugent.be RI Van Rooij, David/A-7938-2014; Baciu, Calin/C-4186-2011; Etiope, Giuseppe/H-3343-2011 OI Van Rooij, David/0000-0003-3633-3344; Baciu, Calin/0000-0002-1142-0620; Etiope, Giuseppe/0000-0001-8614-4221 FU ARES grant from the Innovative Research and Development program at JSC; Romanian CNCS [PN-II-ID-PCE-2011-3-0537]; Astromaterials Research and Exploration Science (ARES) Directorate at Johnson Space Center (JSC) FX The Astromaterials Research and Exploration Science (ARES) Directorate at Johnson Space Center (JSC) provided facilities and support. This work was partially supported by an ARES grant from the Innovative Research and Development program at JSC. The contribution of Dr. Calin Baciu was supported by a grant of Romanian CNCS, Project PN-II-ID-PCE-2011-3-0537. We are also grateful to Dr. J.A. Cartwright, Dr. S.M. Clifford, and an anonymous reviewer for many thoughtful comments which helped us to improve this manuscript. NR 104 TC 2 Z9 2 U1 2 U2 23 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 JUN PY 2013 VL 224 IS 2 SI SI BP 424 EP 432 DI 10.1016/j.icarus.2012.09.018 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162VD UT WOS:000320293200014 ER PT J AU Rice, JL Phoha, VV Robinson, P AF Rice, Justin L. Phoha, Vir V. Robinson, Philip TI Using Mussel-Inspired Self-Organization and Account Proxies to Obfuscate Workload Ownership and Placement in Clouds SO IEEE TRANSACTIONS ON INFORMATION FORENSICS AND SECURITY LA English DT Article DE Distributed systems; animal behavior; multi-agent systems; data privacy; data security; risk analysis AB Recent research has provided evidence indicating how a malicious user could perform coresidence profiling and public-to-private IP mapping to target and exploit customers which share physical resources. The attacks rely on two steps: resource placement on the target's physical machine and extraction. Our proposed solution, in part inspired by mussel self-organization, relies on user account and workload clustering to mitigate coresidence profiling. Users with similar preferences and workload characteristics are mapped to the same cluster. To obfuscate the public-to-private IP map, each cluster is managed and accessed by an account proxy. Each proxy uses one public IP address, which is shared by all clustered users when accessing their instances, and maintains the mapping to private IP addresses. We describe a set of capabilities and attack paths an attacker needs to execute for targeted coresidence, and present arguments to show how our approach disrupts the critical steps in the attack path for most cases. We then perform a risk assessment to determine the likelihood an individual user will be victimized, given that a successful nondirected exploit has occurred. Our results suggest that while possible, this event is highly unlikely. C1 [Rice, Justin L.; Phoha, Vir V.] Louisiana Tech Univ, Dept Comp Sci, Ruston, LA 71272 USA. [Rice, Justin L.] NASA, Goddard Space Flight Ctr, Flight Software Syst Branch, Greenbelt, MD 20771 USA. [Robinson, Philip] SAP Next Business & Technol, Belfast BT3 9DT, Antrim, North Ireland. RP Rice, JL (reprint author), Louisiana Tech Univ, Dept Comp Sci, Ruston, LA 71272 USA. EM jlr060@latech.edu; phoha@latech.edu; philip.robinson@sap.com NR 26 TC 0 Z9 1 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1556-6013 EI 1556-6021 J9 IEEE T INF FOREN SEC JI IEEE Trans. Inf. Forensic Secur. PD JUN PY 2013 VL 8 IS 6 SI SI BP 963 EP 972 DI 10.1109/TIFS.2013.2259158 PG 10 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 155CX UT WOS:000319724100012 ER PT J AU De Lannoy, GJM Reichle, RH Pauwels, VRN AF De Lannoy, Gabrielle J. M. Reichle, Rolf H. Pauwels, Valentijn R. N. TI Global Calibration of the GEOS-5 L-Band Microwave Radiative Transfer Model over Nonfrozen Land Using SMOS Observations SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SURFACE SOIL-MOISTURE; L-MEB MODEL; BRIGHTNESS TEMPERATURES; DATA ASSIMILATION; WATER-CONTENT; BARE FIELD; 1.4 GHZ; EMISSION; VEGETATION; VALIDATION AB A zero-order (tau-omega) microwave radiative transfer model (RTM) is coupled to the Goddard Earth Observing System, version 5 (GEOS-5) catchment land surface model in preparation for the future assimilation of global brightness temperatures (Tb) from the L-band (1.4 GHz) Soil Moisture Ocean Salinity (SMOS) and Soil Moisture Active Passive (SMAP) missions. Simulations using literature values for the RTM parameters result in Tb biases of 10-50 K against SMOS observations. Multiangular SMOS observations during nonfrozen conditions from 1 July 2011 to 1 July 2012 are used to calibrate parameters related to the microwave roughness h, vegetation opacity t and/or scattering albedo v separately for each observed 36-km land grid cell. A particle swarm optimization is used to minimize differences in the long-term (climatological) mean values and standard deviations between SMOS observations and simulations, without attempting to reduce the shorter-term (seasonal to daily) errors. After calibration, global Tb simulations for the validation year (1 July 2010 to 1 July 2011) are largely unbiased for multiple incidence angles and both H and V polarization [e.g., the global average absolute difference is 2.7 K for TbH(42.58), i.e., at 42.58 incidence angle]. The calibrated parameter values depend to some extent on the specific land surface conditions simulated by the GEOS-5 system and on the scale of the SMOS observations, but they also show realistic spatial distributions. Aggregating the calibrated parameter values by vegetation class prior to using them in the RTM maintains low global biases but increases local biases [e.g., the global average absolute difference is 7.1 K for Tb-H(42.58 degrees)]. C1 [De Lannoy, Gabrielle J. M.; Reichle, Rolf H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [De Lannoy, Gabrielle J. M.; Pauwels, Valentijn R. N.] Univ Ghent, Lab Hydrol & Water Management, Ghent, Belgium. RP De Lannoy, GJM (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA. EM gabrielle.delannoy@nasa.gov RI Reichle, Rolf/E-1419-2012; OI Pauwels, Valentijn/0000-0002-1290-9313 FU NASA Soil Moisture Active Passive mission; NASA program on the Science of Terra and Aqua [NNH09ZDA001N-TERRAQUA]; NASA High End Computing Program FX Gabrielle De Lannoy was a research fellow of the Research Foundation Flanders (FWO). Funding for Gabrielle De Lannoy and Rolf Reichle was also provided by the NASA Soil Moisture Active Passive mission and by the NASA program on the Science of Terra and Aqua (NNH09ZDA001N-TERRAQUA). Computing was supported by the NASA High End Computing Program. The first author thanks Niko Verhoest for supporting research abroad. The authors thank Yann Kerr, Patricia de Rosnay, Delphine Leroux, and Ali Mahmoodi for many helpful discussions in the development of this research and Jean-Pierre Wigneron for feedback to this manuscript. We also greatly appreciate the insightful suggestions from three anonymous reviewers. NR 78 TC 31 Z9 31 U1 3 U2 24 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 JUN PY 2013 VL 14 IS 3 BP 765 EP 785 DI 10.1175/JHM-D-12-092.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 162XZ UT WOS:000320300600005 ER PT J AU Li, HY Wigmosta, MS Wu, H Huang, MY Ke, YH Coleman, AM Leung, LR AF Li, Hongyi Wigmosta, Mark S. Wu, Huan Huang, Maoyi Ke, Yinghai Coleman, Andre M. Leung, L. Ruby TI A Physically Based Runoff Routing Model for Land Surface and Earth System Models SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID GENERAL-CIRCULATION MODELS; CLIMATE-CHANGE; RIVER FLOW; WATER; SIMULATION; HYDROLOGY; VELOCITY; COLUMBIA; ALGORITHM; WETLANDS AB A new physically based runoff routing model, called the Model for Scale Adaptive River Transport (MOSART), has been developed to be applicable across local, regional, and global scales. Within each spatial unit, surface runoff is first routed across hillslopes and then discharged along with subsurface runoff into a "tributary subnetwork'' before entering the main channel. The spatial units are thus linked via routing through the main channel network, which is constructed in a scale-consistent way across different spatial resolutions. All model parameters are physically based, and only a small subset requires calibration. MOSART has been applied to the Columbia River basin at 1/16 degrees, 1/88 degrees, 1/4 degrees, and 1/2 degrees spatial resolutions and was evaluated using naturalized or observed streamflow at a number of gauge stations. MOSART is compared to two other routing models widely used with land surface models, the River Transport Model (RTM) in the Community Land Model (CLM) and the Lohmann routing model, included as a postprocessor in the Variable Infiltration Capacity (VIC) model package, yielding consistent performance at multiple resolutions. MOSART is further evaluated using the channel velocities derived from field measurements or a hydraulic model at various locations and is shown to be capable of producing the seasonal variation and magnitude of channel velocities reasonably well at different resolutions. Moreover, the impacts of spatial resolution on model simulations are systematically examined at local and regional scales. Finally, the limitations of MOSART and future directions for improvements are discussed. C1 [Li, Hongyi; Wigmosta, Mark S.; Huang, Maoyi; Ke, Yinghai; Coleman, Andre M.; Leung, L. Ruby] Pacific NW Natl Lab, Richland, WA 99352 USA. [Wu, Huan] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Wu, Huan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Li, HY (reprint author), Pacific NW Natl Lab, 902 Battelle Blvd,POB 999,MSIN K9-33, Richland, WA 99352 USA. EM hongyi.li@pnnl.gov RI Li, Hong-Yi/C-9143-2014; Wu, Huan/K-1003-2013; Huang, Maoyi/I-8599-2012 OI Li, Hong-Yi/0000-0001-5690-3610; Wu, Huan/0000-0003-2920-8860; Huang, Maoyi/0000-0001-9154-9485 FU Department of Energy Biological and Environmental Research (BER) (ESM) and (IAM) programs through the (iESM) and (CSSEF) projects; Platform for Regional Integrated Modeling and Analysis (PRIMA) initiative; U.S. Department of Energy [DE-AC06-76RLO1830] FX This study is supported by the Department of Energy Biological and Environmental Research (BER) Earth System Modeling (ESM) and Integrated Assessment Modeling (IAM) programs through the Integrated Earth System Modeling (iESM) and Climate Science for Sustainable Energy Future (CSSEF) projects. Development of the datasets used in this study is also partly supported by the Platform for Regional Integrated Modeling and Analysis (PRIMA) initiative. In addition, some data and information were provided by the Surface Hydrology Group, University of Washington (http://www.hydro.washington.edu/2860/). We thank Sara Kallio, William Perkins, and Marshall Richmond of PNNL for providing the simulation results from the MASS model. The Pacific Northwest National Laboratory is operated by Battelle for the U.S. Department of Energy under Contract DE-AC06-76RLO1830. NR 61 TC 37 Z9 38 U1 0 U2 49 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 JUN PY 2013 VL 14 IS 3 BP 808 EP 828 DI 10.1175/JHM-D-12-015.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 162XZ UT WOS:000320300600007 ER PT J AU Rebora, N Molini, L Casella, E Comellas, A Fiori, E Pignone, F Siccardi, F Silvestro, F Tanelli, S Parodi, A AF Rebora, N. Molini, L. Casella, E. Comellas, A. Fiori, E. Pignone, F. Siccardi, F. Silvestro, F. Tanelli, S. Parodi, A. TI Extreme Rainfall in the Mediterranean: What Can We Learn from Observations? SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID SEA-SURFACE TEMPERATURE; NUMERICAL SIMULATIONS; PRECIPITATING EVENTS; MOUNTAIN RIDGE; FLASH-FLOOD; MECHANISMS; CONVECTION; HURRICANES; FORECASTS; FLOWS AB Flash floods induced by extreme rainfall events represent one of the most life-threatening phenomena in the Mediterranean. While their catastrophic ground effects are well documented by postevent surveys, the extreme rainfall events that generate them are still difficult to observe properly. Being able to collect observations of such events will help scientists to better understand and model these phenomena. The recent flash floods that hit the Liguria region (Italy) between the end of October and beginning of November 2011 give us the opportunity to use the measurements available from a large number of sensors, both ground based and spaceborne, to characterize these events. In this paper, the authors analyze the role of the key ingredients (e.g., unstable air masses, moist low-level jets, steep orography, and a slow-evolving synoptic pattern) for severe rainfall processes over complex orography. For the two Ligurian events, this role has been analyzed through the available observations (e.g., Meteosat Second Generation, Moderate Resolution Imaging Spectroradiometer, the Italian Radar Network mosaic, and the Italian rain gauge network observations). The authors then address the possible role of sea-atmosphere interactions and propose a characterization of these events in terms of their predictability. C1 [Rebora, N.; Molini, L.; Casella, E.; Comellas, A.; Fiori, E.; Pignone, F.; Siccardi, F.; Silvestro, F.; Parodi, A.] CIMA Res Fdn, I-17100 Savona, Italy. [Casella, E.; Comellas, A.; Fiori, E.; Pignone, F.; Siccardi, F.] Univ Genoa, Genoa, Italy. [Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Rebora, N (reprint author), CIMA Res Fdn, Via Magliotto 2, I-17100 Savona, Italy. EM nicola.rebora@cimafoundation.org FU Italian Civil Protection Department; Regione Liguria; National Aeronautics and Space Administration; Precipitation Measurement Missions program; FP7 DRIHM (Distributed Research Infrastructure for Hydro-Meteorology) project [283568] FX This work is supported by Italian Civil Protection Department and by Regione Liguria. We acknowledge Regione Liguria and Regione Piemonte for providing us with the data of the regional meteorological observation networks. We acknowledge the Italian Civil Protection Department for providing us with the Italian Radar Network data. We acknowledge the LIMET association for providing us with the data from their meteorological observation network. We acknowledge the Institute of Atmospheric Sciences and Climate-Satellite Oceanography Group (ISAC-GOS) for providing us with the CNR MED sea surface temperature data. We are very grateful to the meteorologists and the hydrologists of the Meteo-Hydrologic Centre of Liguria Region for many useful discussions. The portion of work carried out by Simone Tanelli was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with National Aeronautics and Space Administration; support from the Precipitation Measurement Missions program is gratefully acknowledged. Nicola Rebora and Antonio Parodi would like to acknowledge the support by the FP7 DRIHM (Distributed Research Infrastructure for Hydro-Meteorology, 2011-2015) project (Contract 283568). The authors also thank Garvin Cummings for help in revising this paper. NR 36 TC 36 Z9 36 U1 0 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD JUN PY 2013 VL 14 IS 3 BP 906 EP 922 DI 10.1175/JHM-D-12-083.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 162XZ UT WOS:000320300600012 ER PT J AU Yu, SS Pearson, JC Drouin, BJ AF Yu, Shanshan Pearson, John C. Drouin, Brian J. TI Terahertz spectroscopy of water in its second triad SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE High temperature water; THz spectroscopy; DC discharge ID VIBRATIONAL-STATES; ROTATIONAL LEVELS; ENERGY-LEVELS; LINE; (H2O)-O-16; MOLECULE; SPECTRA AB Terahertz absorption spectroscopy was employed to measure rotational transitions of water in its second triad 3v(2), v(1) + v(2) and v(3) + v(2). Highly excited water molecules were created with a DC discharge, which allowed observation of transitions with lower state energies up to 5939 cm(-1). In the 0.5-2.0 THz region, 38 pure rotational transitions in the second triad were observed with MW accuracy for the first time. Additionally, 91 new rotational and ro-vibrational transitions within the ground state, v(2), and the first triad (2v(2), v(1) and v(3)) were measured with multiplier chains covering the 1.3-2.0 THz region. (C) 2013 Elsevier Inc. All rights reserved. C1 [Yu, Shanshan; Pearson, John C.; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yu, SS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM shanshan.yu@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU National Aeronautics and Space Administration; California Institute of Technology. Government FX We would like to thank Laurent Coudert for providing his linelist of the second triad rotational transitions before his publication. The research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Copyright 2013 California Institute of Technology. Government sponsorship acknoledged. NR 14 TC 2 Z9 2 U1 0 U2 26 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 JUN PY 2013 VL 288 BP 7 EP 10 DI 10.1016/j.jms.2013.03.011 PG 4 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 163QA UT WOS:000320350800002 ER PT J AU Cohen, EA Drouin, BJ AF Cohen, Edward A. Drouin, Brian J. TI Submillimeter wave spectrum of sulfuric acid, H2SO4 SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE H2SO4; Sulfuric acid; Submillimeter spectrum; Rotational constants ID ROTATIONAL SPECTRUM; DIPOLE-MOMENT AB The submillimeter spectrum of H2SO4 has been measured in selected regions up to 655.6 GHz. The new measurements have been combined with available literature rotational data in a merged fit. This has resulted in an improved and extended set of rotational and centrifugal constants which accurately describe the spectrum well into the submillimeter region. (C) 2013 Elsevier Inc. All rights reserved. C1 [Cohen, Edward A.; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cohen, EA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Edward.A.Cohen@jpl.nasa.gov FU National Aeronautics and Space Administration FX We thank Kenneth R. Leopold and Carolyn S. Brauer for providing Fourier transform microwave data prior to publication. This work was done at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. NR 9 TC 1 Z9 1 U1 1 U2 9 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 JUN PY 2013 VL 288 BP 67 EP 69 DI 10.1016/j.jms.2013.04.008 PG 3 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 163QA UT WOS:000320350800011 ER PT J AU Ohman, T Preeden, U AF Ohman, Teemu Preeden, Ulla TI Shock metamorphic features in quartz grains from the Saarijarvi and Soderfjarden impact structures, Finland SO METEORITICS & PLANETARY SCIENCE LA English DT Review ID PLANAR DEFORMATION FEATURES; WESTERN FINLAND; CRATERING RECORD; FENNOSCANDIA; LAMELLAE; DEPOSITS; TVAREN; VAASA; ROCKS AB Shock metamorphic features at the Saarijarvi (D>2km) and Soderfjarden (D=6.5km) structures in Finland have so far only been studied tentatively, although both are considered to be proven impact structures. This work presents the first detailed universal stage study of planar deformation features (PDFs), feather feature lamellae (FFL), and planar fractures (PFs) in quartz grains from a polymict impact breccia dike from Soderfjarden, and from sedimentary crater-fill rocks from Saarijarvi. Planar microstructures, particularly PDFs, are very rare and poorly developed or preserved in Saarijarvi, whereas in Soderfjarden they are much more common and well defined. Miller-Bravais indices of the planar microstructures in both Saarijarvi and Soderfjarden are indicative of relatively low-shock pressure but high shear conditions, only compatible with an impact origin for these structures. Although a Proterozoic age for Saarijarvi cannot be ruled out, the observations of shock features throughout the sedimentary crater-fill sequence and a brecciated sedimentary dike below the crater floor are more consistent with a Lower Cambrian (or younger) impact age. C1 [Ohman, Teemu] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77508 USA. [Ohman, Teemu] NASA, Ctr Lunar Sci & Explorat, Lunar Sci Inst, Washington, DC USA. [Ohman, Teemu] Univ Oulu, Dept Geosci, FI-90014 Oulu, Finland. [Ohman, Teemu] Univ Oulu, Dept Phys, Planetol Grp, FI-90014 Oulu, Finland. [Preeden, Ulla] Univ Tartu, Dept Geol, EE-50411 Tartu, Estonia. [Preeden, Ulla] Polva Cty Govt, EE-63308 Polva, Estonia. RP Ohman, T (reprint author), Univ Space Res Assoc, Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77508 USA. EM ohman@lpi.usra.edu OI Ohman, Teemu/0000-0001-8214-841X FU Magnus Ehrnrooth Foundation; Finnish Graduate School in Geology and Vilho; Yrjo and Kalle Vaisala Foundation; NASA [NNX08AC28A]; NASA Lunar Science Institute [NNA09DB33A] FX T. Ohman would like to thank the following people for providing data, samples, comments, thought-provoking discussions, help in various forms, and collaboration on different aspects of Soderfjarden and particularly Saarijarvi studies, only a small part of which have been directly touched upon in this report, but which have greatly affected the development of ideas of the formation and evolution of these structures: A. Abels, D. D. Badjukov, P. Eden, S. Elo, B. M. French, M. J. Holma, J. Kohonen, T. Korja, G. Y. Kramer, D. A. Kring, M. Kurimo, M. Lehtinen, J. Moilanen, A. L. Nahm, K. Nuutinen, L. J. Pesonen, J. Plado, J. Raitala, K. Strand, K. Tiensuu, P. Tuisku, P. Turunen, A. Uutela, M. Vaarma, S. Vishnevsky, and J. Vuollo. U. Preeden thanks J. Kirs and K. Kirsimae. We acknowledge the detailed and constructive reviews by M. Poelchau and L. Ferriere, as well as comments by associate editor G. Osinski, which greatly improved the manuscript. Magnus Ehrnrooth Foundation is thanked for funding the logging of Saarijarvi drill cores, which was crucial for Saarijarvi geology to start making any sense. Early parts of this research were made possible by funding from the Finnish Graduate School in Geology and Vilho, Yrjo and Kalle Vaisala Foundation, whereas the later work was supported by NASA under the LPI Cooperative Agreement NNX08AC28A, and NASA Lunar Science Institute contract NNA09DB33A (PI David A. Kring). This is LPI Contribution 1724. NR 97 TC 2 Z9 2 U1 2 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUN PY 2013 VL 48 IS 6 BP 955 EP 975 DI 10.1111/maps.12112 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 164EQ UT WOS:000320392100002 ER PT J AU Lindgren, P Lee, MR Sofe, MR Zolensky, ME AF Lindgren, Paula Lee, Martin R. Sofe, Mahmood R. Zolensky, Michael E. TI Clasts in the CM2 carbonaceous chondrite Lonewolf Nunataks 94101: Evidence for aqueous alteration prior to complex mixing SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID KRYMKA LL3.1 CHONDRITE; PARENT BODY; CI CHONDRITES; FOSSIL MICROMETEORITES; MINERALOGY; METEORITE; ORIGIN; PHYLLOSILICATES; HOWARDITES; CARBONATES AB Clasts in the CM2 carbonaceous chondrite Lonewolf Nunataks (LON) 94101 have been characterized using scanning and transmission electron microscopy and electron microprobe analysis to determine their degrees of aqueous alteration, and the timing of alteration relative to incorporation of clasts into the host. The provenance of the clasts, and the mechanism by which they were incorporated and mixed with their host material are also considered. Results show that at least five distinct types of clasts occur in LON 94101, of which four have been aqueously altered to various degrees and one is largely anhydrous. The fact that they have had different alteration histories implies that the main part of aqueous activity occurred prior to the mixing and assimilation of the clasts with their host. Further, the presence of such a variety of clasts suggests complex mixing in a dynamic environment involving material from various sources. Two of the clasts, one containing approximately 46 vol% carbonate and the other featuring crystals of pyrrhotite up to approximately 1mm in size, are examples of unusual lithologies and indicate concentration of chemical elements in discrete areas of the parent body(ies), possibly by flow of aqueous solutions. C1 [Lindgren, Paula; Lee, Martin R.; Sofe, Mahmood R.] Univ Glasgow, Sch Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland. [Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Lindgren, P (reprint author), Univ Glasgow, Sch Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland. EM paula.lindgren@glasgow.ac.uk RI Lee, Martin/D-9169-2011 OI Lee, Martin/0000-0002-6004-3622 FU Science and Technology Facilities Council (STFC); NASA Cosmochemistry Program FX We are grateful to the Meteorite Working Group for loan of the thin sections. We thank Peter Chung, Brian Miller, and Colin How at the University of Glasgow, and Chris Hayward at the University of Edinburgh for skilled technical support, and Science and Technology Facilities Council (STFC) for funding. MEZ was supported by the NASA Cosmochemistry Program. NR 64 TC 7 Z9 7 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUN PY 2013 VL 48 IS 6 BP 1074 EP 1090 DI 10.1111/maps.12133 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 164EQ UT WOS:000320392100010 ER PT J AU Ball, P Caillat, T AF Ball, Philip Caillat, Thierry TI Thermoelectric heat recovery could boost auto fuel economy SO MRS BULLETIN LA English DT Editorial Material C1 [Caillat, Thierry] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM p.ball@btinternet.com NR 0 TC 3 Z9 3 U1 2 U2 12 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0883-7694 J9 MRS BULL JI MRS Bull. PD JUN PY 2013 VL 38 IS 6 BP 446 EP 447 DI 10.1557/mrs.2013.138 PG 2 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 159FA UT WOS:000320029200008 ER PT J AU Cliver, EW Richardson, IG Ling, AG AF Cliver, E. W. Richardson, I. G. Ling, A. G. TI Solar Drivers of 11-yr and Long-Term Cosmic Ray Modulation SO SPACE SCIENCE REVIEWS LA English DT Review DE Sun; Solar Cycle; Solar Wind; Coronal Mass Ejections; High-speed Streams; Galactic Cosmic Rays; Cosmic Ray Modulation ID CORONAL MASS EJECTIONS; HELIOSPHERIC CURRENT SHEET; DEPENDENT DRIFT MODEL; MERGED INTERACTION REGIONS; NONAXISYMMETRIC OPEN FLUX; WIND MAGNETIC-FIELD; VOYAGER-2 OBSERVATIONS; GEOMAGNETIC-ACTIVITY; PARTICLE DRIFT; TILT ANGLE AB In the current paradigm for the modulation of galactic cosmic rays (GCRs), diffusion is taken to be the dominant process during solar maxima while drift dominates at minima. Observations during the recent solar minimum challenge the pre-eminence of drift at such times. In 2009, the similar to 2 GV GCR intensity measured by the Newark neutron monitor increased by similar to 5% relative to its maximum value two cycles earlier even though the average tilt angle in 2009 was slightly larger than that in 1986 (similar to 20A degrees vs. similar to 14A degrees), while solar wind B was significantly lower (similar to 3.9 nT vs. similar to 5.4 nT). A decomposition of the solar wind into high-speed streams, slow solar wind, and coronal mass ejections (CMEs; including post-shock flows) reveals that the Sun transmits its message of changing magnetic field (diffusion coefficient) to the heliosphere primarily through CMEs at solar maximum and high-speed streams at solar minimum. Long-term reconstructions of solar wind B are in general agreement for the similar to 1900-present interval and can be used to reliably estimate GCR intensity over this period. For earlier epochs, however, a recent Be-10-based reconstruction covering the past similar to 10(4) years shows nine abrupt and relatively short-lived drops of B to a parts per thousand(2)0 nT, with the first of these corresponding to the Sporer minimum. Such dips are at variance with the recent suggestion that B has a minimum or floor value of similar to 2.8 nT. A floor in solar wind B implies a ceiling in the GCR intensity (a permanent modulation of the local interstellar spectrum) at a given energy/rigidity. The 30-40% increase in the intensity of 2.5 GV electrons observed by Ulysses during the recent solar minimum raises an interesting paradox that will need to be resolved. C1 [Cliver, E. W.] USA, Space Vehicles Directorate, Res Lab, Hanscom Afb, MA USA. [Richardson, I. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Richardson, I. G.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. [Ling, A. G.] Atmospher & Environm Res Inc, Lexington, MA USA. RP Cliver, EW (reprint author), USA, Space Vehicles Directorate, Res Lab, Hanscom Afb, MA USA. EM afrl.rvb.pa@hanscom.af.mil OI Richardson, Ian/0000-0002-3855-3634 FU AFRL [FA8718-05-C-0036] FX It is a pleasure to thank Jurg Beer, Bernd Heber, Randy Jokipii, Jozsef Kota, Frank McDonald, Harm Moraal, and Rudolf von Steiger for organizing this timely and stimulating workshop. In addition, we are grateful to Marius Potgieter for constructive criticism. A.G.L. acknowledges support from AFRL contract FA8718-05-C-0036. NR 75 TC 22 Z9 22 U1 0 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 JUN PY 2013 VL 176 IS 1-4 BP 3 EP 19 DI 10.1007/s11214-011-9746-3 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 163ZX UT WOS:000320379200002 ER PT J AU Wiedenbeck, ME AF Wiedenbeck, M. E. TI Cosmic-Ray Energy Spectra and Time Variations in the Local Interstellar Medium: Constraints and Uncertainties SO SPACE SCIENCE REVIEWS LA English DT Review DE Cosmic rays; Interstellar medium; Solar modulation ID DIFFUSE GAMMA-RAYS; IONIZATION RATE; SUPERNOVA-REMNANTS; SOLAR MODULATION; MOLECULAR CLOUDS; PROPAGATION; ELECTRONS; ACCELERATION; SPECTROMETER; HELIOSPHERE AB The spectra of galactic cosmic rays that are observed inside the heliosphere result from the interaction of the spectra present in the local interstellar medium with the structured but turbulent magnetic field carried by the solar wind. Observational tests of solar modulation theory depend on comparisons between spectra inside and outside the heliosphere. Our knowledge of the local interstellar spectra are indirect, using extrapolations of interplanetary spectra measured at high energies where solar modulation effects are minimal and modeling of the physical processes that occur during particle acceleration and transport in the interstellar medium. The resulting estimates of the interstellar spectra can also be checked against observations of the effects that cosmic rays have on the chemistry of the interstellar medium and on the production of the diffuse galactic gamma-ray background. I review the present understanding of the local galactic cosmic-ray spectra, emphasizing the constraints set by observations and the uncertainties that remain. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. RP Wiedenbeck, ME (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. EM mark.e.wiedenbeck@jpl.nasa.gov FU NASA at Caltech; JPL [NNX08AI11G] FX I wish to thank the organizers of the April 2010 ISSI workshop on Cosmic Rays in the Heliosphere II for putting together a very interesting multidisciplinary meeting. I am grateful to Richard Leske for his careful reading of the manuscript. This research was supported, in part, by NASA at Caltech and JPL under grant NNX08AI11G. NR 55 TC 2 Z9 2 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD JUN PY 2013 VL 176 IS 1-4 BP 35 EP 46 DI 10.1007/s11214-011-9778-8 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 163ZX UT WOS:000320379200004 ER PT J AU Richardson, JD Burlaga, LF AF Richardson, J. D. Burlaga, L. F. TI The Solar Wind in the Outer Heliosphere and Heliosheath SO SPACE SCIENCE REVIEWS LA English DT Review DE Solar wind; Termination shock; Heliosheath; Heliopause; Pickup ions; Interstellar neutral atoms; Anomalous cosmic rays ID COSMIC-RAY MODULATION; INTERSTELLAR MAGNETIC-FIELD; TERMINATION SHOCK; VOYAGER-2 OBSERVATIONS; GEOMAGNETIC-ACTIVITY; DISTANT HELIOSPHERE; INTERACTION REGIONS; ION DISTRIBUTIONS; PICKUP PROTONS; SLOWDOWN AB The solar wind environment has a large influence on the transport of cosmic rays. This chapter discusses the observations of the solar wind plasma and magnetic field in the outer heliosphere and the heliosheath. In the supersonic solar wind, interaction regions with large magnetic fields form barriers to cosmic ray transport. This effect, the "CR-B" relationship, has been quantified and is shown to be valid everywhere inside the termination shock (TS). In the heliosheath, this relationship breaks down, perhaps because of a change in the nature of the turbulence. Turbulence is compressive in the heliosheath, whereas it was non-compressive in the solar wind. The plasma pressure in the outer heliosphere is dominated by the pickup ions which gain most of the flow energy at the TS. The heliosheath plasma and magnetic field are highly variable on scales as small as ten minutes. The plasma flow turns away from the nose roughly as predicted, but the radial speeds at Voyager 1 are much less than those at Voyager 2, which is not understood. Despite predictions to the contrary, magnetic reconnection is not an important process in the inner heliosheath with only one observed occurrence to date. C1 [Richardson, J. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Richardson, JD (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jdr@space.mit.edu; lburlagahsp@verizon.net FU NASA from JPL [959203] FX The work at MIT was supported under NASA contract 959203 from JPL to MIT. NR 67 TC 9 Z9 9 U1 2 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JUN PY 2013 VL 176 IS 1-4 BP 217 EP 235 DI 10.1007/s11214-011-9825-5 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 163ZX UT WOS:000320379200016 ER PT J AU Kukreja, SL AF Kukreja, Sunil L. TI Data-Driven Model Development for the SuperSonic SemiSpan Transport SO AIAA JOURNAL LA English DT Article ID PROPER ORTHOGONAL DECOMPOSITION; ORDER; SYSTEMS; IDENTIFICATION; REDUCTION; SIMULATION; FLOW AB We investigate two common approaches to model development for robust control synthesis in the aerospace community; namely, reduced-order aeroservoelastie modeling based on structural finite-element and computational-fluid-dynamics-based aerodynamic models and a data-driven system-identification procedure. It is shown via analysis of experimental SuperSonic SemiSpan Transport wind-tunnel data that, using a system-identification approach, it is possible to estimate a model at a fixed Mach number that is parsimonious and robust across varying dynamic pressures while the numerical reduced-order model offers significantly less predicative capability. C1 NASA, Dryden Flight Res Ctr, Struct Dynam Grp, Edwards AFB, CA 93523 USA. RP Kukreja, SL (reprint author), NASA, Dryden Flight Res Ctr, Struct Dynam Grp, Mail Stop T-47, Edwards AFB, CA 93523 USA. EM Sunil.L.Kukreja@nasa.gov NR 54 TC 0 Z9 0 U1 1 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD JUN PY 2013 VL 51 IS 6 BP 1333 EP 1341 DI 10.2514/1.J051721 PG 9 WC Engineering, Aerospace SC Engineering GA 154CB UT WOS:000319648000006 ER PT J AU Nielsen, EJ Diskin, B AF Nielsen, Eric J. Diskin, Boris TI Discrete Adjoint-Based Design for Unsteady Turbulent Flows on Dynamic Overset Unstructured Grids SO AIAA JOURNAL LA English DT Article ID NAVIER-STOKES EQUATIONS; SENSITIVITY-ANALYSIS; COMPLEX-VARIABLES; OPTIMIZATION; MESHES; ADAPTATION; ALGORITHM; IMPLICIT AB A discrete adjoint-based design methodology for unsteady turbulent flows on three-dimensional dynamic overset unstructured grids is formulated, implemented, and verified. The methodology supports both compressible and incompressible flows and is amenable to massively parallel computing environments. The approach provides a general framework for performing highly efficient and discretely consistent sensitivity analysis for problems involving arbitrary combinations of overset unstructured grids that may be static, undergoing rigid or deforming motions, or any combination thereof. General parent child motions are also accommodated, and the accuracy of the implementation is established using an independent verification based on a complex-variable approach. The methodology is used to demonstrate aerodynamic optimizations of a wind-turbine geometry, a biologically inspired flapping wing, and a complex helicopter configuration subject to trimming constraints. The objective function for each problem is successfully reduced, and all specified constraints are satisfied. C1 [Nielsen, Eric J.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA. [Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23681 USA. RP Nielsen, EJ (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, MS 128, Hampton, VA 23681 USA. FU Fundamental Aeronautics Project within the NASA Aeronautics Research Mission Directorate; NASA [NNL07AA23C, NNL09AA00A] FX The first author is supported by the subsonic rotary-wing element of the Fundamental Aeronautics Project within the NASA Aeronautics Research Mission Directorate. The second author acknowledges the support from NASA through contract NNL07AA23C and cooperative agreement NNL09AA00A. Both authors wish to thank Robert Biedron of NASA Langley Research Center and Nail Yamaleev of North Carolina A&T State University for many helpful conversations pertaining to the current work. The enabling contributions of Elizabeth Lee-Rausch and William Jones of NASA Langley Research Center in the areas of grid generation and parameterization are very much appreciated. The work has also greatly benefitted from the high-performance computing research conducted by Dana Hammond of NASA Langley Research Center. Discussions with David Darmofal, Qiqi Wang, and Josh Krakos of the Massachusetts Institute of Technology (MIT) and Yuping Sun of Vestas Wind Systems were very useful. Ralph Noack of Pennsylvania State University is acknowledged for his support and assistance in using his overset grid libraries. Thanks are due to C. Eric Lynch of Naval Air Systems Command for providing the mesh used for the wind-turbine example. The authors are grateful to John Moore of MIT and the staff of the Air Force Research Laboratory for providing the mesh and problem definition for the flapping-wing case. NR 70 TC 15 Z9 15 U1 2 U2 13 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD JUN PY 2013 VL 51 IS 6 BP 1355 EP 1373 DI 10.2514/1.J051859 PG 19 WC Engineering, Aerospace SC Engineering GA 154CB UT WOS:000319648000008 ER PT J AU Kaul, UK AF Kaul, Upender K. TI Stability Enhanced High-Order Hyperviscosity-Based Shock Capturing Algorithm SO AIAA JOURNAL LA English DT Article ID FINITE-DIFFERENCE SCHEMES; FLOWS; SIMULATION; RESOLUTION; MESHES; WAVES C1 NASA Ames Res Ctr, Appl Modeling Simulat Branch, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA. RP Kaul, UK (reprint author), NASA Ames Res Ctr, Appl Modeling Simulat Branch, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA. FU NASA FX The author would like to thank Peter Coen and Don Durston for their interest and support of the development of the new flow solver, EDLFLOW, under the aegis of the Supersonics/EDL Project of the NASA Fundamental Aeronautics Program. The author would also like to thank Chuck Player for subsequent support of this work under the Hypersonics/ADT Project of the Fundamental Aeronautics Program. The geometry definition for the tension cone LAD provided by Ian Clark of Georgia Institute of Technology is gratefully acknowledged. The review of this manuscript by Shishir Pandya and Jasim Ahmad of NASA Ames Research Center is thankfully acknowledged. NR 33 TC 1 Z9 1 U1 1 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD JUN PY 2013 VL 51 IS 6 BP 1516 EP 1521 DI 10.2514/1.J051704 PG 6 WC Engineering, Aerospace SC Engineering GA 154CB UT WOS:000319648000021 ER PT J AU Dorodnitsyn, A AF Dorodnitsyn, A. TI Probing AGN unification with radiation hydrodynamics simulations of dusty obscuring winds SO HIGH ENERGY DENSITY PHYSICS LA English DT Article DE Acceleration of particles; Galaxies: active; Hydrodynamics; Methods: numerical ID ACTIVE NUCLEUS; OBSCURATION; NGC-1068; TORUS AB Observational properties of active galactic nucleus are essentially influenced by their winds. The illumination of a parsec-scale, geometrically thin, dusty accretion disk by X-rays, and UV radiation leads to the conversion of such radiation into IR. In result the disk becomes geometrically thick due to pressure of the IR radiation on dust, and eventually develops a rigorous IR-driven accretion disk wind. Here we present the results from the radiation hydrodynamics simulations that take into account the conversion of X-rays into IR with the latter calculated in a flux-limited diffusion approximation. We show that when AGN luminosity, exceeds 0.1L(edd), the outflowing dusty wind provides the obscuration with IR pressure on dust playing a major role. The outer dense and cold part of the flow provides obscuration while the inner hot, and photoionized has properties similar to those of a warm absorber flow. At luminosities <0.1L(edd) episodes of the outflow are followed by extended periods when the wind switches to slow accretion. (c) 2013 Elsevier B.V. All rights reserved. C1 [Dorodnitsyn, A.] NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dorodnitsyn, A.] Univ Maryland, Dept Astron CRESST, College Pk, MD 20742 USA. RP Dorodnitsyn, A (reprint author), Univ Maryland, Dept Astron CRESST, College Pk, MD 20742 USA. EM dorodnitsyn@gmail.com FU NASA Goddard Space Flight Center; NASA; NASA Astrophysics Theory Program [10-ATP10-0171] FX This research was supported by an appointment at the NASA Goddard Space Flight Center, administered by CRESST/UMD through a contract with NASA, and by grants from the NASA Astrophysics Theory Program 10-ATP10-0171. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1574-1818 J9 HIGH ENERG DENS PHYS JI High Energy Density Phys. PD JUN PY 2013 VL 9 IS 2 BP 277 EP 279 DI 10.1016/j.hedp.2012.12.015 PG 3 WC Physics, Fluids & Plasmas SC Physics GA 158EN UT WOS:000319952300008 ER PT J AU Leal-Sevillano, CA Reck, TJ Jung-Kubiak, C Chattopadhyay, G Ruiz-Cruz, JA Montejo-Garai, JR Rebollar, JM AF Leal-Sevillano, Carlos A. Reck, Theodore J. Jung-Kubiak, Cecile Chattopadhyay, Goutam Ruiz-Cruz, Jorge A. Montejo-Garai, Jose R. Rebollar, Jesus M. TI Silicon Micromachined Canonical E-Plane and H-Plane Bandpass Filters at the Terahertz Band SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE Deep reactive ion etching (DRIE); filter; micromachining; terahertz; WR-15 AB In this letter, several bandpass filters operating in the WR-1.5 band (500 to 750 GHz) are presented. The deep reactive ion etching (DRIE) silicon micromachining process is used for the fabrication of the filters. Two canonical filter topologies based on E- and H-plane are implemented. The work presented here has two specific objectives: a) to get important fabrication process parameters, such as tolerances, vertical angles, surface roughness, and repeatability and b) to validate the proper working of the waveguide filters in the terahertz band. These filters do not have any tuning element. Experimental results show better than 10 dB return loss and approximately 1 and 2.5 dB insertion loss (for 6% fractional bandwidth) for the E- and H-plane topology, respectively. The obtained results are in agreement with fabrication tolerances of 2 mu m and vertical angles deviations up to 3 degrees. C1 [Leal-Sevillano, Carlos A.; Montejo-Garai, Jose R.; Rebollar, Jesus M.] Univ Politecn Madrid, Dept Electromagnetismo & Teoria Circuitos, ETSI Telecomunicac, E-28040 Madrid, Spain. [Reck, Theodore J.; Jung-Kubiak, Cecile; Chattopadhyay, Goutam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ruiz-Cruz, Jorge A.] Univ Autonoma Madrid, Escuela Politecn Super, E-28049 Madrid, Spain. RP Leal-Sevillano, CA (reprint author), Univ Politecn Madrid, Dept Electromagnetismo & Teoria Circuitos, ETSI Telecomunicac, E-28040 Madrid, Spain. EM caleal@etc.upm.es RI Ruiz-Cruz, Jorge/C-8159-2014 OI Ruiz-Cruz, Jorge/0000-0003-3909-8263 FU National Aeronautincs and Space Administration; Universidad Politecnica de Madrid; Spanish government [TEC2010-17795]; CONSOLIDER [CSD2008-00068] FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, under a contract with the National Aeronautincs and Space Administration. This work was supported in part by the Spanish government program TEC2010-17795, the CONSOLIDER CSD2008-00068 and a Ph.D. grant from Universidad Politecnica de Madrid. NR 11 TC 14 Z9 14 U1 0 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD JUN PY 2013 VL 23 IS 6 BP 288 EP 290 DI 10.1109/LMWC.2013.2258097 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 160PM UT WOS:000320131600006 ER PT J AU Jiang, XA Maloney, ED Li, JLF Waliser, DE AF Jiang, Xianan Maloney, Eric D. Li, Jui-Lin F. Waliser, Duane E. TI Simulations of the Eastern North Pacific Intraseasonal Variability in CMIP5 GCMs SO JOURNAL OF CLIMATE LA English DT Article ID MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODELS; AMERICAN-MONSOON; BOREAL SUMMER; MIDSUMMER DROUGHT; AGCM SIMULATIONS; CLIMATE MODELS; PART I; SYSTEM; MJO AB As a key component of tropical atmospheric variability, intraseasonal variability (ISV) over the eastern North Pacific Ocean (ENP) exerts pronounced influences on regional weather and climate. Since general circulation models (GCMs) are essential tools for prediction and projection of future climate, current model deficiencies in representing this important variability leave us greatly disadvantaged in studies and prediction of climate change. In this study, the authors have assessed model fidelity in representing ENP ISV by analyzing 16 GCMs participating in phase 5 of the Coupled Model Intercomparison Project (CMIP5). Among the 16 CMIP5 GCMs examined in this study, only seven GCM scapture the spatial pattern of the leading ENP ISV mode relatively well, although even these GCMs exhibit biases in simulating ISV amplitude. Analyses indicate that model fidelity in representing ENP ISV is closely associated with the ability to simulate a realistic summer mean state. The presence of westerly or weak mean easterly winds over the ENP warm pool region could be conducive to more realistic simulations of the ISV. One hypothesis to explain this relationship is that a realistic mean state could produce the correct sign of surface flux anomalies relative to the ISV convection, which helps to destabilize local intraseasonal disturbances. The projected changes in characteristics of ENP ISV under the representative concentration pathway 8.5 (RCP8.5) projection scenario are also explored based on simulations from three CMIP5 GCMs. Results suggest that, in a future climate, the amplitude of ISV could be enhanced over the southern part of the ENP while reduced over the northern ENP off the coast of Mexico/Central America and the Caribbean. C1 [Jiang, Xianan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Jiang, Xianan; Li, Jui-Lin F.; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Maloney, Eric D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Jiang, XA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-300, Pasadena, CA 91109 USA. EM xianan@jifresse.ucla.edu RI Jiang, Xianan/A-2283-2012; Maloney, Eric/A-9327-2008 OI Maloney, Eric/0000-0002-2660-2611 FU NOAA MAPP program as part of the CMIP5 Task Force; National Science Foundation's Climate and Large-Scale Dynamics Program [ATM-0934285, AGS-0946911, AGS-1025584]; National Aeronautics and Space Administration; [NA09OAR4310191]; [NA11OAR4310086]; [NA08OAR4320893 7]; [NA08OAR4320893 14] FX The authors acknowledge the support of the NOAA MAPP program as part of the CMIP5 Task Force. Work was supported under grants NA09OAR4310191 and NA11OAR4310086 (X.J.), and NA08OAR4320893 #7 and #14 (E.D.M.). We also acknowledge support from the National Science Foundation's Climate and Large-Scale Dynamics Program under Awards ATM-0934285 (X.J.), AGS-0946911, and AGS-1025584 (E.D.M.). Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Global ocean heat flux and evaporation products were provided by the WHOI OAFlux project (http://oaflux.whoi.edu). NR 44 TC 11 Z9 12 U1 2 U2 25 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 JUN PY 2013 VL 26 IS 11 BP 3489 EP 3510 DI 10.1175/JCLI-D-12-00526.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 155HT UT WOS:000319739300001 ER PT J AU Colas, F Capet, X Mcwilliams, JC Li, ZJ AF Colas, Francois Capet, Xavier Mcwilliams, James C. Li, Zhijin TI Mesoscale Eddy Buoyancy Flux and Eddy-Induced Circulation in Eastern Boundary Currents SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID CALIFORNIA CURRENT SYSTEM; OCEAN CIRCULATION; MIXED-LAYER; SURFACE VORTEX; PART I; MODELS; DYNAMICS; PARAMETERIZATION; TRANSPORT; VELOCITY AB A dynamical interpretation is made of the mesoscale eddy buoyancy fluxes in the Eastern Boundary Currents off California and Peru-Chile, based on regional equilibrium simulations. The eddy fluxes are primarily shoreward and upward across a swath several hundred kilometers wide in the upper ocean; as such they serve to balance mean offshore air-sea heating and coastal upwelling. In the stratified interior the eddy fluxes are consistent with the adiabatic hypothesis associated with a mean eddy-induced velocity advecting mean buoyancy and tracers. Furthermore, with a suitable gauge choice, the horizontal fluxes are almost entirely aligned with the mean horizontal buoyancy gradient, consistent with the advective parameterization scheme of Gent and McWilliams. The associated diffusivity kappa is surface intensified, matching the vertical stratification profile. The fluxes span the across-shore band of high eddy energy, but their alongshore structure is unresolved because of sampling limitations. In the surface layer the eddy flux is significantly diabatic with a shallow eddy-induced circulation cell and downgradient lateral diapycnal flux. The dominant eddy generation process is baroclinic instability, but there are significant regional differences between the upwelling systems in the flux and kappa that are not consistent with simple instability theory. C1 [Colas, Francois; Mcwilliams, James C.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Capet, Xavier] Lab Phys Oceans, Plouzane, France. [Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Colas, F (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM francois@atmos.ucla.edu RI Colas, Francois/B-4920-2012 OI Colas, Francois/0000-0002-5859-6586 FU Office of Naval Research [N00014- 08-1-0597]; National Science Foundation [ATM-0747533] FX This research was supported by the Office of Naval Research, Grant N00014- 08-1-0597 and the National Science Foundation, Grant ATM-0747533. The computations were made at the National Center for Supercomputing Applications. NR 65 TC 18 Z9 18 U1 0 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD JUN PY 2013 VL 43 IS 6 BP 1073 EP 1095 DI 10.1175/JPO-D-11-0241.1 PG 23 WC Oceanography SC Oceanography GA 161AN UT WOS:000320162300001 ER PT J AU Gopalswamy, N Xie, H Makela, P Yashiro, S Akiyama, S Uddin, W Srivastava, AK Joshi, NC Chandra, R Manoharan, PK Mahalakshmi, K Dwivedi, VC Jain, R Awasthi, AK Nitta, NV Aschwanden, MJ Choudhary, DP AF Gopalswamy, N. Xie, H. Maekelae, P. Yashiro, S. Akiyama, S. Uddin, W. Srivastava, A. K. Joshi, N. C. Chandra, R. Manoharan, P. K. Mahalakshmi, K. Dwivedi, V. C. Jain, R. Awasthi, A. K. Nitta, N. V. Aschwanden, M. J. Choudhary, D. P. TI Height of shock formation in the solar corona inferred from observations of type II radio bursts and coronal mass ejections SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Coronal mass ejections; Shock; Type II radio bursts ID NEAR-SUN; WAVES AB Employing coronagraphic and EUV observations close to the solar surface made by the Solar Terrestrial Relations Observatory (STEREO) mission, we determined the heliocentric distance of coronal mass ejections (CMEs) at the starting time of associated metric type II bursts. We used the wave diameter and leading edge methods and measured the CME heights for a set of 32 metric type II bursts from solar cycle 24. We minimized the projection effects by making the measurements from a view that is roughly orthogonal to the direction of the ejection. We also chose image frames close to the onset times of the type II bursts, so no extrapolation was necessary. We found that the CMEs were located in the heliocentric distance range from 1.20 to 1.93 solar radii (Rs), with mean and median values of 1.43 and 1.38 Rs, respectively. We conclusively find that the shock formation can occur at heights substantially below 1.5 Rs. In a few cases, the CME height at type II onset was close to 2 Rs. In these cases, the starting frequency of the type II bursts was very low, in the range 25-40 MHz, which confirms that the shock can also form at larger heights. The starting frequencies of metric type II bursts have a weak correlation with the measured CME/shock heights and are consistent with the rapid decline of density with height in the inner corona. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Gopalswamy, N.; Xie, H.; Maekelae, P.; Yashiro, S.; Akiyama, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Uddin, W.; Srivastava, A. K.; Joshi, N. C.] ARIES Nainital, Naini Tal 263129, India. [Chandra, R.] Kumaun Univ, Naini Tal 263129, India. [Manoharan, P. K.; Mahalakshmi, K.; Dwivedi, V. C.] TIFR NCRA Radio Astron Ctr, Ootacamund 643001, India. [Jain, R.; Awasthi, A. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Nitta, N. V.; Aschwanden, M. J.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Choudhary, D. P.] Calif State Univ Northridge, Northridge, CA 91330 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov RI Srivastava, Abhishek /C-5017-2012; Awasthi, Arun/H-5596-2016 OI Awasthi, Arun/0000-0001-5313-1125 FU NASA's LWS TRT program; ISRO's CAWSES-India Program FX This study was conducted as a part of the Indo-US Science and Technology Forum's Joint Center on Solar Eruptive Events. We acknowledge the use of radio dynamic spectra made available on line at Culgoora, Hiraiso, Green Bank, and the RSTN data from NGDC. This work was supported by NASA's LWS TRT program. PKM was partly supported by ISRO's CAWSES-India Program. NR 19 TC 26 Z9 26 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD JUN 1 PY 2013 VL 51 IS 11 BP 1981 EP 1989 DI 10.1016/j.asr.2013.01.006 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 152RV UT WOS:000319549700002 ER PT J AU Grillmair, CJ Cutri, R Masci, FJ Conrow, T Sesar, B Eisenhardt, PRM Wright, EL AF Grillmair, Carl J. Cutri, Roc Masci, Frank J. Conrow, Tim Sesar, Branimir Eisenhardt, Peter R. M. Wright, Edward L. TI DETECTION OF A NEARBY HALO DEBRIS STREAM IN THE WISE AND 2MASS SURVEYS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: halo; Galaxy: structure; globular clusters: general; globular clusters: individual (NGC 288) ID SMALL-MAGELLANIC-CLOUD; GLOBULAR-CLUSTERS; SKY SURVEY; MILKY-WAY; TIDAL TAILS; STELLAR STREAM; STAR STREAM; PALOMAR 5; TELESCOPE; EVOLUTION AB Combining the Wide-Field Infrared Survey Explorer All-Sky Release with the Two Micron All Sky Survey Point Source Catalog, we detect a nearby, moderately metal-poor stellar debris stream spanning 24 degrees across the southern sky. The stream, which we designate Alpheus, is at an estimated distance of similar to 1.9 kpc. Its position, orientation, width, estimated metallicity, and, to some extent, its distance, are in approximate agreement with what one might expect of the leading tidal tail of the southern globular cluster NGC 288. C1 [Grillmair, Carl J.] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Cutri, Roc; Masci, Frank J.; Conrow, Tim; Sesar, Branimir] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Sesar, Branimir] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wright, Edward L.] Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. RP Grillmair, CJ (reprint author), Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM carl@ipac.caltech.edu; roc@ipac.caltech.edu; fmasci@ipac.caltech.edu; tim@ipac.caltech.edu; bsesar@astro.caltech.edu; peter.r.eisenhardt@jpl.nasa.gov; wright@astro.ucla.edu FU NASA [NNX12AI57G]; National Aeronautics and Space Administration; National Science Foundation FX We gratefully acknowledge several probing questions by an anonymous referee which helped us to improve and clarify the manuscript. We also thank S. van den Bergh for suggesting a new source of stream designations. This paper is based upon work supported in part by NASA under award No. NNX12AI57G.This publication makes use of data products from the Wide-Field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. It also makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 41 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2013 VL 769 IS 2 AR L23 DI 10.1088/2041-8205/769/2/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151JR UT WOS:000319457300005 ER PT J AU Pavan, J Vinas, AF Yoon, PH Ziebell, LF Gaelzer, R AF Pavan, J. Vinas, A. F. Yoon, P. H. Ziebell, L. F. Gaelzer, R. TI SOLAR WIND STRAHL BROADENING BY SELF-GENERATED PLASMA WAVES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE diffusion; instabilities; interplanetary medium; plasmas; solar wind; waves ID THERMAL NOISE SPECTROSCOPY; SUPRATHERMAL ELECTRONS; INTERPLANETARY MEDIUM; WHISTLER WAVES; HALO; TEMPERATURE; DENSITY; CORONA; CORE AB This Letter reports on the results of numerical simulations which may provide a possible explanation for the strahl broadening during quiet solar conditions. The relevant processes involved in the broadening are due to kinetic quasi-linear wave-particle interaction. Making use of static analytical electron distribution in an inhomogeneous field, it is found that self-generated electrostatic waves at the plasma frequency, i.e., Langmuir waves, are capable of scattering the strahl component, resulting in energy and pitch-angle diffusion that broadens its velocity distribution significantly. The present theoretical results provide an alternative or complementary explanation to the usual whistler diffusion scenario, suggesting that self-induced electrostatic waves at the plasma frequency might play a key role in broadening the solar wind strahl during quiet solar conditions. C1 [Pavan, J.; Gaelzer, R.] Univ Fed Pelotas, Pelotas, Brazil. [Vinas, A. F.] NASA GSFC, Greenbelt, MD 20771 USA. [Yoon, P. H.] UMD, IPST, College Pk, MD USA. [Ziebell, L. F.] Univ Fed Rio Grande do Sul, Porto Alegre, RS, Brazil. [Yoon, P. H.] KHU, SSR, Yongin, South Korea. RP Pavan, J (reprint author), Univ Fed Pelotas, Pelotas, Brazil. EM joel.pavan@ufpel.edu.br; adolfo.vinas@nasa.gov; yoonp@umd.edu; luiz.ziebell@ufrgs.br RI Yoon, Peter/E-2395-2013; Ziebell, Luiz/N-7334-2014; Gaelzer, Rudi/E-4437-2013 OI Gaelzer, Rudi/0000-0001-5851-7959 FU Brazilian agency CNPq; Brazilian agency FAPERGS; NASA; NSF [AGS1242331]; WCU grant from the Korean Ministry of Education, Science, and Technology [R31-10016] FX The research carried out at UFPEL and UFRGS was supported by Brazilian agencies CNPq and FAPERGS. A. F. V. thanks NASA for funding support received by the Cluster mission and PEACE experiment at the Goddard Space Flight Center. The research at the University of Maryland was supported by NSF grant AGS1242331. The research carried out at Kyung Hee University, Korea, was supported by WCU grant R31-10016 from the Korean Ministry of Education, Science, and Technology. NR 33 TC 10 Z9 10 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2013 VL 769 IS 2 AR L30 DI 10.1088/2041-8205/769/2/L30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151JR UT WOS:000319457300012 ER PT J AU Zemcov, M Blain, A Cooray, A Bethermin, M Bock, J Clements, DL Conley, A Conversi, L Dowell, CD Farrah, D Glenn, J Griffin, M Halpern, M Jullo, E Kneib, JP Marsden, G Nguyen, HT Oliver, SJ Richard, J Roseboom, IG Schulz, B Scott, D Shupe, DL Smith, AJ Valtchanov, I Viero, M Wang, L Wardlow, J AF Zemcov, M. Blain, A. Cooray, A. Bethermin, M. Bock, J. Clements, D. L. Conley, A. Conversi, L. Dowell, C. D. Farrah, D. Glenn, J. Griffin, M. Halpern, M. Jullo, E. Kneib, J. -P. Marsden, G. Nguyen, H. T. Oliver, S. J. Richard, J. Roseboom, I. G. Schulz, B. Scott, Douglas Shupe, D. L. Smith, A. J. Valtchanov, I. Viero, M. Wang, L. Wardlow, J. TI HerMES: A DEFICIT IN THE SURFACE BRIGHTNESS OF THE COSMIC INFRARED BACKGROUND DUE TO GALAXY CLUSTER GRAVITATIONAL LENSING SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmic background radiation ID DARK-MATTER; MAGNIFICATION; EMISSION; Z=0.2; CORES; DUST; MASS AB We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after removing detected sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I-250 mu m > 0.69(-0.03)(+0.03)(stat.)(-0.06)(+0.11)(sys.) MJy sr(-1), with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB. C1 [Zemcov, M.; Cooray, A.; Bock, J.; Dowell, C. D.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Viero, M.] CALTECH, Pasadena, CA 91125 USA. [Zemcov, M.; Bock, J.; Dowell, C. D.; Nguyen, H. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Blain, A.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bethermin, M.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu, CNRS, F-91191 Gif Sur Yvette, France. [Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France. [Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Conversi, L.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain. [Farrah, D.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Glenn, J.] Univ Colorado, CASA UCB 389, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Griffin, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Halpern, M.; Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Jullo, E.; Kneib, J. -P.] Aix Marseille Univ, CNRS, LAM, UMR7326, F-13388 Marseille, France. [Kneib, J. -P.] Observ Sauverny, EPFL, Astrophys Lab, CH-1290 Versoix, Switzerland. [Richard, J.] Univ Lyon 1, Ctr Rech Astron Lyon, F-69230 St Genis Laval, France. [Richard, J.] Ecole Normale Super Lyon, UMR 5574, CNRS, F-69007 Lyon, France. [Roseboom, I. G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Schulz, B.; Shupe, D. L.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. RP Zemcov, M (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM zemcov@caltech.edu RI Wardlow, Julie/C-9903-2015; Kneib, Jean-Paul/A-7919-2015; OI Wardlow, Julie/0000-0003-2376-8971; Kneib, Jean-Paul/0000-0002-4616-4989; Scott, Douglas/0000-0002-6878-9840; Bethermin, Matthieu/0000-0002-3915-2015 FU NASA; CSA (Canada); NAOC (China); CEA; CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC; UKSA (UK); NASA (USA) FX Support for this work was provided by NASA.; SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including: University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). NR 30 TC 7 Z9 7 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2013 VL 769 IS 2 AR L31 DI 10.1088/2041-8205/769/2/L31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151JR UT WOS:000319457300013 ER PT J AU Gu, GJ Adler, RF AF Gu, Guojun Adler, Robert F. TI Interdecadal variability/long-term changes in global precipitation patterns during the past three decades: global warming and/or pacific decadal variability? SO CLIMATE DYNAMICS LA English DT Article ID 20TH-CENTURY CLIMATE VARIATIONS; SPATIOTEMPORAL STRUCTURE; PART II; REANALYSES; TRENDS; CYCLE AB This study explores how global precipitation and tropospheric water vapor content vary on the interdecadal/long-term time scale during past three decades (1988-2010 for water vapor), in particular to what extent the spatial structures of their variations relate to changes in surface temperature. EOF analyses of satellite-based products indicate that the first two modes of global precipitation and columnar water vapor content anomalies are in general related to the El Nio-Southern oscillation. The spatial patterns of their third modes resemble the corresponding linear fits/trends estimated at each grid point, which roughly represent the interdecadal/long-term changes happening during the same time period. Global mean sea surface temperature (SST) and land surface temperature have increased during the past three decades. However, the water vapor and precipitation patterns of change do not reflect the pattern of warming, in particular in the tropical Pacific basin. Therefore, other mechanisms in addition to global warming likely exist to account for the spatial structures of global precipitation changes during this time period. An EOF analysis of longer-record (1949-2010) SST anomalies within the Pacific basin (60(o)N-60(o)S) indicates the existence of a strong climate regime shift around 1998/1999, which might be associated with the Pacific decadal variability (PDV) as suggested in past studies. Analyses indicate that the observed linear changes/trends in both precipitation and tropospheric water vapor during 1988-2010 seem to result from a combined impact of global mean surface warming and the PDV shift. In particular, in the tropical central-eastern Pacific, a band of increases along the equator in both precipitation and water vapor sandwiched by strong decreases south and north of it are likely caused by the opposite effects from global-mean surface warming and PDV-related, La Nia-like cooling in the tropical central-eastern Pacific. This narrow band of precipitation increase could also be considered an evidence for the influence of global mean surface warming. C1 [Gu, Guojun; Adler, Robert F.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Gu, Guojun] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gu, GJ (reprint author), NASA, Atmospheres Lab, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. EM Guojun.Gu-1@nasa.gov FU NASA Energy and Water-cycle Study (NEWS) program FX The RSS-SSM/I and RSS-SSMIS columnar water vapor data were downloaded from http://www.remss.com. The ERSST data set (v3b) was downloaded from the NOAA-NCDC website at http://www.ncdc.noaa.gov/ersst/. The NASA-GISS global surface temperature anomaly product was downloaded from its website at http://data.giss.nasa.gov/. This research is supported under the NASA Energy and Water-cycle Study (NEWS) program. NR 44 TC 15 Z9 15 U1 2 U2 39 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD JUN PY 2013 VL 40 IS 11-12 BP 3009 EP 3022 DI 10.1007/s00382-012-1443-8 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 149ZU UT WOS:000319360800025 ER PT J AU Wild, M Folini, D Schar, C Loeb, N Dutton, EG Konig-Langlo, G AF Wild, Martin Folini, Doris Schaer, Christoph Loeb, Norman Dutton, Ellsworth G. Koenig-Langlo, Gert TI The global energy balance from a surface perspective SO CLIMATE DYNAMICS LA English DT Article DE Earth Radiation Budget; Surface energy balance; Global climate models; Global energy balance; Surface/Satellite observations; CMIP5/IPCC-AR5 model evaluation ID GENERAL-CIRCULATION MODELS; LONGWAVE IRRADIANCE UNCERTAINTY; RADIATION BUDGET EXPERIMENT; SHORTWAVE IRRADIANCE; ATMOSPHERE RADIATION; CLIMATE RESEARCH; SOLAR-RADIATION; ERA-INTERIM; UPPER-OCEAN; FLUXES AB In the framework of the global energy balance, the radiative energy exchanges between Sun, Earth and space are now accurately quantified from new satellite missions. Much less is known about the magnitude of the energy flows within the climate system and at the Earth surface, which cannot be directly measured by satellites. In addition to satellite observations, here we make extensive use of the growing number of surface observations to constrain the global energy balance not only from space, but also from the surface. We combine these observations with the latest modeling efforts performed for the 5th IPCC assessment report to infer best estimates for the global mean surface radiative components. Our analyses favor global mean downward surface solar and thermal radiation values near 185 and 342 Wm(-2), respectively, which are most compatible with surface observations. Combined with an estimated surface absorbed solar radiation and thermal emission of 161 and 397 Wm(-2), respectively, this leaves 106 Wm(-2) of surface net radiation available globally for distribution amongst the non-radiative surface energy balance components. The climate models overestimate the downward solar and underestimate the downward thermal radiation, thereby simulating nevertheless an adequate global mean surface net radiation by error compensation. This also suggests that, globally, the simulated surface sensible and latent heat fluxes, around 20 and 85 Wm(-2) on average, state realistic values. The findings of this study are compiled into a new global energy balance diagram, which may be able to reconcile currently disputed inconsistencies between energy and water cycle estimates. C1 [Wild, Martin; Folini, Doris; Schaer, Christoph] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. [Loeb, Norman] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Dutton, Ellsworth G.] NOAA, ESRL, R GMD, Boulder, CO 80305 USA. [Koenig-Langlo, Gert] Alfred Wegener Inst, D-27570 Bremerhaven, Germany. RP Wild, M (reprint author), ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland. EM martin.wild@env.ethz.ch RI Konig-Langlo, Gert/K-5048-2012; Schar, Christoph/A-1033-2008; Wild, Martin/J-8977-2012 OI Konig-Langlo, Gert/0000-0002-6100-4107; Schar, Christoph/0000-0002-4171-1613; FU National Centre for Competence in Climate Research (NCCR Climate) of the Swiss National Science Foundation as part of the NCCR Project HyClim; Office of Science, U.S. Department of Energy FX This study is supported by the National Centre for Competence in Climate Research (NCCR Climate) of the Swiss National Science Foundation as part of the NCCR Project HyClim. We are grateful to Prof. Atsumu Ohmura for numerous discussions and for his leadership in the establishment of GEBA and BSRN. We highly acknowledge Barbara Schar for the design of the global energy balance figure. We would like to thank Dr. Guido Muller for processing the BSRN data and Dr. Urs Beyerle and Dr. Thierry Corti for all their efforts to download the immense CMIP5 dataset. We acknowledge the international modeling groups for providing their data for analysis, the Program for Climate Model Diagnosis and Intercomparison (PCMDI) for collecting and archiving the model data, the JSC/CLIVAR Working Group on Coupled Modelling (WGCM) and their Coupled Model Intercomparison Project (CMIP) and Climate Simulation Panel for organizing the model data analysis activity, and the IPCC WG1 TSU for technical support. The IPCC Data Archive at Lawrence Livermore National Laboratory is supported by the Office of Science, U.S. Department of Energy. We would like to take this opportunity to acknowledge many hard working site scientists, as listed in http://hdl.handle.net/10013/epic.40092.d001. BSRN data used in this study are available at http://dx.doi.org/10.1594/PANGAEA.792618. We dedicate this study to our dear friend and colleague Ellsworth G. Dutton, who passed away the day this paper was accepted. His enthusiasm and devotion as BSRN project manager over 20 years was invaluable for the success of BSRN. NR 76 TC 86 Z9 89 U1 9 U2 110 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD JUN PY 2013 VL 40 IS 11-12 BP 3107 EP 3134 DI 10.1007/s00382-012-1569-8 PG 28 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 149ZU UT WOS:000319360800030 ER PT J AU Tam, CKW Parrish, SA Envia, E Chien, EW AF Tam, Christopher K. W. Parrish, Sarah A. Envia, Edmane Chien, Eugene W. TI Physical processes influencing acoustic radiation from jet engine inlets SO JOURNAL OF FLUID MECHANICS LA English DT Article DE acoustics; aeroacoustics ID TURBOFAN NOISE RADIATION; BOUNDARY-CONDITIONS; COMPUTATIONAL AEROACOUSTICS; FLOW; SIMULATION; PATTERNS; FLIGHT; DUCT AB Numerical simulations of acoustic radiation from a jet engine inlet are performed using advanced computational aeroacoustics algorithms and high-quality numerical boundary treatments. As a model of modern commercial jet engine inlets, the inlet geometry of the NASA Source Diagnostic Test is used. Fan noise consists of tones and broadband sound. This investigation considers the radiation of tones associated with upstream-propagating duct modes. The primary objective is to identify the dominant physical processes that determine the directivity of the radiated sound. Two such processes have been identified. They are acoustic diffraction and refraction. Diffraction is the natural tendency for an acoustic duct mode to follow a curved solid surface as it propagates. Refraction is the turning of the direction of propagation of a duct mode by mean flow gradients. Parametric studies on the changes in the directivity of radiated sound due to variations in forward flight Mach number, duct mode frequency, azimuthal mode number and radial mode number are carried out. It is found there is a significant difference in directivity for the radiation of the same duct mode from an engine inlet when operating in static condition versus one in forward flight. It will be shown that the large change in directivity is the result of the combined effects of diffraction and refraction. C1 [Tam, Christopher K. W.; Parrish, Sarah A.] Florida State Univ, Dept Math, Tallahassee, FL 32306 USA. [Envia, Edmane] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Chien, Eugene W.] Goodrich Aerostruct Grp, Chula Vista, CA 91910 USA. RP Tam, CKW (reprint author), Florida State Univ, Dept Math, Tallahassee, FL 32306 USA. EM tam@math.fsu.edu NR 48 TC 0 Z9 0 U1 2 U2 9 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 EI 1469-7645 J9 J FLUID MECH JI J. Fluid Mech. PD JUN PY 2013 VL 725 BP 152 EP 194 DI 10.1017/jfm.2013.181 PG 43 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 152DQ UT WOS:000319511200007 ER PT J AU Ueyama, R Gerber, EP Wallace, JM Frierson, DMW AF Ueyama, Rei Gerber, Edwin P. Wallace, John M. Frierson, Dargan M. W. TI The Role of High-Latitude Waves in the Intraseasonal to Seasonal Variability of Tropical Upwelling in the Brewer-Dobson Circulation SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID MEAN MERIDIONAL CIRCULATION; GENERAL-CIRCULATION; LOWER STRATOSPHERE; MIDDLE ATMOSPHERE; ANNUAL CYCLE; TROPOPAUSE TEMPERATURES; DOWNWARD CONTROL; PLANETARY-WAVES; TROPOSPHERE; MODEL AB The forcing of tropical upwelling in the Brewer-Dobson circulation (BDC) on intraseasonal to seasonal time scales is investigated in integrations of an idealized general circulation model, ECMWF Interim ReAnalysis, and lower-stratospheric temperature measurements from the (Advanced) Microwave Sounding Unit, with a focus on the extended boreal winter season. Enhanced poleward eddy heat fluxes in the high latitudes (45 degrees-90 degrees N) at the 100-hPa level are associated with anomalous tropical cooling and anomalous warming on the poleward side of the polar night jet at the 70-hPa level and above. In both the model and the observations, planetary waves entering the stratosphere at high latitudes propagate equatorward to the subtropics and tropics at levels above 70 hPa over an approximately 10-day period, exerting a force at sufficiently low latitudes to modulate the tropical upwelling in the upper branch of the BDC, even on time scales longer than the radiative relaxation time scale of the lower stratosphere. To the extent that they force the BDC via downward as opposed to sideways control, planetary waves originating in high latitudes contribute to the seasonally varying climatological mean and the interannual variability of tropical upwelling at the 70-hPa level and above. Their influence upon the strength of the tropical upwelling, however, diminishes rapidly with depth below 70 hPa. In particular, tropical upwelling at the cold-point tropopause, near 100 hPa, appears to be modulated by variations in the strength of the lower branch of the BDC. C1 [Ueyama, Rei] NASA, Div Earth Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gerber, Edwin P.] NYU, Courant Inst Math Sci, Ctr Atmosphere Ocean Sci, New York, NY USA. [Wallace, John M.; Frierson, Dargan M. W.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. RP Ueyama, R (reprint author), NASA, Div Earth Sci, Ames Res Ctr, Mail Stop 245-5, Moffett Field, CA 94035 USA. EM rei.ueyama@nasa.gov RI Frierson, Dargan/F-1763-2010; OI Frierson, Dargan/0000-0001-8952-5644; Gerber, Edwin/0000-0002-6010-6638 FU NOAA Climate and Global Change Program; NSF [1122989]; division of Atmospheric and Geospace Sciences [0938325, 0846641, 0936059]; NASA [NNX09AH73G]; NOAA [NA08OAR4310725] FX MSU/AMSU data are produced by Remote Sensing Systems and sponsored by the NOAA Climate and Global Change Program. We thank two anonymous reviewers for their thoughtful comments and suggestions on the manuscript. This work was partially funded by NSF Climate Dynamics Program Office Grant 1122989 and the division of Atmospheric and Geospace Sciences Grants 0938325, 0846641, and 0936059; NASA Grant NNX09AH73G; and NOAA Grant NA08OAR4310725. R. Ueyama also thanks Dr. Leonhard Pfister and the NASA Postdoctoral Program for support. NR 55 TC 18 Z9 18 U1 0 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD JUN PY 2013 VL 70 IS 6 BP 1631 EP 1648 DI 10.1175/JAS-D-12-0174.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 154IP UT WOS:000319668400008 ER PT J AU Gruppioni, C Pozzi, F Rodighiero, G Delvecchio, I Berta, S Pozzetti, L Zamorani, G Andreani, P Cimatti, A Ilbert, O Le Floc'h, E Lutz, D Magnelli, B Marchetti, L Monaco, P Nordon, R Oliver, S Popesso, P Riguccini, L Roseboom, I Rosario, DJ Sargent, M Vaccari, M Altieri, B Aussel, H Bongiovanni, A Cepa, J Daddi, E Dominguez-Sanchez, H Elbaz, D Schreiber, NF Genzel, R Iribarrem, A Magliocchetti, M Maiolino, R Poglitsch, A Garcia, AP Sanchez-Portal, M Sturm, E Tacconi, L Valtchanov, I Amblard, A Arumugam, V Bethermin, M Bock, J Boselli, A Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chanial, P Clements, DL Conley, A Cooray, A Dowell, CD Dwek, E Eales, S Franceschini, A Glenn, J Griffin, M Hatziminaoglou, E Ibar, E Isaak, K Ivison, RJ Lagache, G Levenson, L Lu, N Madden, S Maffei, B Mainetti, G Nguyen, HT O'Halloran, B Page, MJ Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rigopoulou, D Rowan-Robinson, M Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Vigroux, L Wang, L Wright, G Xu, CK Zemcov, M Bardelli, S Carollo, M Contini, T Le Fevre, O Lilly, S Mainieri, V Renzini, A Scodeggio, M Zucca, E AF Gruppioni, C. Pozzi, F. Rodighiero, G. Delvecchio, I. Berta, S. Pozzetti, L. Zamorani, G. Andreani, P. Cimatti, A. Ilbert, O. Le Floc'h, E. Lutz, D. Magnelli, B. Marchetti, L. Monaco, P. Nordon, R. Oliver, S. Popesso, P. Riguccini, L. Roseboom, I. Rosario, D. J. Sargent, M. Vaccari, M. Altieri, B. Aussel, H. Bongiovanni, A. Cepa, J. Daddi, E. Dominguez-Sanchez, H. Elbaz, D. Schreiber, N. Foerster Genzel, R. Iribarrem, A. Magliocchetti, M. Maiolino, R. Poglitsch, A. Perez Garcia, A. Sanchez-Portal, M. Sturm, E. Tacconi, L. Valtchanov, I. Amblard, A. Arumugam, V. Bethermin, M. Bock, J. Boselli, A. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chanial, P. Clements, D. L. Conley, A. Cooray, A. Dowell, C. D. Dwek, E. Eales, S. Franceschini, A. Glenn, J. Griffin, M. Hatziminaoglou, E. Ibar, E. Isaak, K. Ivison, R. J. Lagache, G. Levenson, L. Lu, N. Madden, S. Maffei, B. Mainetti, G. Nguyen, H. T. O'Halloran, B. Page, M. J. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rigopoulou, D. Rowan-Robinson, M. Schulz, B. Scott, D. Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Vigroux, L. Wang, L. Wright, G. Xu, C. K. Zemcov, M. Bardelli, S. Carollo, M. Contini, T. Le Fevre, O. Lilly, S. Mainieri, V. Renzini, A. Scodeggio, M. Zucca, E. TI The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z similar or equal to 4 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: luminosity function; mass function; galaxies: starburst; cosmology: observations; infrared: galaxies ID STAR-FORMING GALAXIES; DEEP-FIELD-SOUTH; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES; REDSHIFT SURVEY; GOODS-SOUTH; MU-M; PHOTOMETRIC REDSHIFTS; FORMATION HISTORY AB We exploit the deep and extended far-IR data sets (at 70, 100 and 160 mu m) of the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 mu m, to derive the evolution of the rest-frame 35-, 60-, 90-and total infrared (IR) luminosity functions (LFs) up to z similar to 4. We detect very strong luminosity evolution for the total IR LF (L-IR alpha (1 + z)(3.55 +/- 0.10) up to z similar to 2, and. (1 + z) 1.62 similar to 0.51 at 2 < z less than or similar to 4) combined with a density evolution ( (1 + z)-0.57 +/- 0.22 up to z similar to 1 and. (1 + z)-3.92 +/- 0.34 at 1 < z less than or similar to 4). In agreement with previous findings, the IR luminosity density (.IR) increases steeply to z similar to 1, then flattens between z similar to 1 and z similar to 3 to decrease at z similar to 3. Galaxies with different spectral energy distributions, masses and specific star formation rates (SFRs) evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to.IR. Galaxies occupying the well-established SFR-stellar mass main sequence (MS) are found to dominate both the total IR LF and.IR at all redshifts, with the contribution from off-MS sources (= 0.6 dex above MS) being nearly constant (similar to 20 per cent of the total IR) and showing no significant signs of increase with increasing z over the whole 0.8 < z < 2.2 range. Sources with mass in the range 10 = log(M/M-circle dot) = 11 are found to dominate the total IR LF, with more massive galaxies prevailing at the bright end of the high-z (greater than or similar to 2) LF. A two-fold evolutionary scheme for IR galaxies is envisaged: on the one hand, a starburst-dominated phase in which the Super Massive Black Holes (SMBH) grows and is obscured by dust (possibly triggered by a major merging event), is followed by an AGN-dominated phase, then evolving towards a local elliptical. On the other hand, moderately star-forming galaxies containing a low-luminosity AGN have various properties suggesting they are good candidates for systems in a transition phase preceding the formation of steady spiral galaxies. C1 [Gruppioni, C.; Pozzetti, L.; Zamorani, G.; Dominguez-Sanchez, H.; Bardelli, S.; Zucca, E.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Pozzi, F.; Delvecchio, I.; Cimatti, A.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Rodighiero, G.; Marchetti, L.; Vaccari, M.; Franceschini, A.; Mainetti, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Berta, S.; Lutz, D.; Magnelli, B.; Nordon, R.; Popesso, P.; Rosario, D. J.; Schreiber, N. Foerster; Genzel, R.; Poglitsch, A.; Sturm, E.; Tacconi, L.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Andreani, P.; Iribarrem, A.; Hatziminaoglou, E.; Mainieri, V.] ESO, D-85748 Garching, Germany. [Ilbert, O.; Boselli, A.; Buat, V.; Burgarella, D.; Le Fevre, O.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Le Floc'h, E.; Riguccini, L.; Sargent, M.; Aussel, H.; Daddi, E.; Elbaz, D.; Bethermin, M.; Chanial, P.; Madden, S.; Panuzzo, P.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Marchetti, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Monaco, P.] Univ Trieste, Dipartimento Fis, Sez Astron, I-34131 Trieste, Italy. [Oliver, S.; Roseboom, I.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Roseboom, I.; Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Bellville, South Africa. [Altieri, B.; Perez Garcia, A.; Sanchez-Portal, M.; Valtchanov, I.] ESA Herschel Sci Ctr, E-28692 Villafranca, Spain. [Bongiovanni, A.; Cepa, J.; Dominguez-Sanchez, H.; Castro-Rodriguez, N.; Perez-Fournon, I.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain. [Iribarrem, A.] Univ Fed Rio de Janeiro, Observ Valongo, BR-21941 Rio De Janeiro, Brazil. [Magliocchetti, M.] INAF IFSI, I-00133 Rome, Italy. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Amblard, A.] NASA, Ames Res Ctr, Moett Field, CA 94035 USA. [Bock, J.; Cooray, A.; Dowell, C. D.; Levenson, L.; Lu, N.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Castro-Rodriguez, N.; Perez-Fournon, I.] Univ La Laguna ULL, Dept Astrofis, E-38205 San Cristobal la Laguna, Spain. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Clements, D. L.; O'Halloran, B.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, 3Astrophys Grp, London SW7 2AZ, England. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dwek, E.] NASA, Observ Cosmol Lab, Code 665, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eales, S.; Griffin, M.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Ibar, E.; Ivison, R. J.; Wright, G.] UK Astron Technol Ctr, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Isaak, K.] ESTEC SRE SA, ESA Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. [Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Pearson, C. P.; Rigopoulou, D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vigroux, L.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Carollo, M.; Lilly, S.] Swiss Fed Inst Technol ETH Honggerberg, Inst Astron, CH-8093 Zurich, Switzerland. [Contini, T.] Univ Toulouse, CNRS, Inst Rech Astrophys & Plantol, F-31400 Toulouse, France. [Renzini, A.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Scodeggio, M.] INAF IASF Milano, I-20133 Milan, Italy. RP Gruppioni, C (reprint author), INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. EM carlotta.gruppioni@oabo.inaf.it RI Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; Daddi, Emanuele/D-1649-2012; Bongiovanni, Angel/J-6176-2012; amblard, alexandre/L-7694-2014; Bardelli, Sandro/O-9369-2015; Zucca, Elena/O-9396-2015; Ivison, R./G-4450-2011; OI Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scodeggio, Marco/0000-0002-2282-5850; Pozzetti, Lucia/0000-0001-7085-0412; Magliocchetti, Manuela/0000-0001-9158-4838; Daddi, Emanuele/0000-0002-3331-9590; amblard, alexandre/0000-0002-2212-5395; Bardelli, Sandro/0000-0002-8900-0298; Zucca, Elena/0000-0002-5845-8132; Ivison, R./0000-0001-5118-1313; Gruppioni, Carlotta/0000-0002-5836-4056 FU national funding agencies: CSA (Canada); national funding agencies: NAOC (China); CEA; CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC; UKSA (UK); NASA (USA); University of Trieste [FRA2009]; [PRIN- INAF 1.06.09.05]; [ASI- INAF I00507/1]; [I005110] FX PACS has been developed by a consortium of institutes led by MPE (Germany) and including: UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/ OAA/OAP/OAT, LENS, SISSA (Italy); and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA- PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by CardiffUniv. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, Univ. Padua (Italy); IAC (Spain); StockholmObservatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). CG and FP acknowledge financial contribution from the contracts PRIN- INAF 1.06.09.05 and ASI- INAF I00507/1 and I005110. PM thanks the University of Trieste for the grant FRA2009. The authors thank an anonymous referee for the helpful comments that greatly improved the quality of the paper. NR 138 TC 106 Z9 105 U1 1 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 1 BP 23 EP 52 DI 10.1093/mnras/stt308 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600023 ER PT J AU Siwak, M Rucinski, SM Matthews, JM Kuschnig, R Guenther, DB Moffat, AFJ Rowe, JF Sasselov, D Weiss, WW AF Siwak, Michal Rucinski, Slavek M. Matthews, Jaymie M. Kuschnig, Rainer Guenther, David B. Moffat, Anthony F. J. Rowe, Jason F. Sasselov, Dimitar Weiss, Werner W. TI Photometric variability in FU Ori and Z CMa as observed by MOST SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: individual: FU Ori; stars: individual: Z CMa ID Z-CANIS-MAJORIS; T TAURI STAR; SYSTEM Z CMA; AU-SCALE; ORIONIS OBJECTS; 2008 OUTBURST; DISK; SPECTROSCOPY; COMPANION; COMPONENT AB Photometric observations obtained by the MOST satellite were used to characterize optical small-scale variability of the young stars FU Ori and Z CMa. Wavelet analysis for FU Ori reveals the possible existence of several 2-9 d quasi-periodic features occurring nearly simultaneously; they may be interpreted as plasma parcels or other localized disc heterogeneities revolving at different Keplerian radii in the accretion disc. Their periods may shorten slowly which may be due to spiralling in of individual parcels towards the inner disc radius, estimated at 4.8 +/- 0.2 R-circle dot. Analysis of additional multicolour data confirms the previously obtained relation between variations in the B - V colour index and the V magnitude. In contrast to the FU Ori results, the oscillation spectrum of Z CMa does not reveal any periodicities with the wavelet spectrum possibly dominated by outburst of the Herbig Be component. C1 [Siwak, Michal] Cracov Pedag Univ, Mt Suhora Astron Observ, PL-30084 Krakow, Poland. [Rucinski, Slavek M.] Univ Toronto, Deparntment Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guenther, David B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Siwak, M (reprint author), Cracov Pedag Univ, Mt Suhora Astron Observ, Ul Podchorazych 2, PL-30084 Krakow, Poland. EM siwak@nac.oa.uj.edu.pl FU Canadian Space Agency; Natural Sciences and Engineering Research Council of Canada; FQRNT (Quebec); Austrian Science Funds [P22691-N16] FX The Natural Sciences and Engineering Research Council of Canada supports the research of DBG, JMM, AFJM and SMR. Additional support for AFJM comes from FQRNT (Quebec). RK is supported by the Canadian Space Agency and WWW is supported by the Austrian Science Funds (P22691-N16). NR 37 TC 4 Z9 4 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 1 BP 194 EP 199 DI 10.1093/mnras/stt441 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600033 ER PT J AU Schmidt, KB Rix, HW da Cunha, E Brammer, GB Cox, TJ van Dokkum, P Schreiber, NMF Franx, M Fumagalli, M Jonsson, P Lundgren, B Maseda, MV Momcheva, I Nelson, EJ Skelton, RE van der Wel, A Whitaker, KE AF Schmidt, Kasper B. Rix, Hans-Walter da Cunha, Elisabete Brammer, Gabriel B. Cox, Thomas J. van Dokkum, Pieter Schreiber, Natascha M. Foerster Franx, Marijn Fumagalli, Mattia Jonsson, Patrik Lundgren, Britt Maseda, Michael V. Momcheva, Ivelina Nelson, Erica J. Skelton, Rosalind E. van der Wel, Arjen Whitaker, Katherine E. TI The spatial extent and distribution of star formation in 3D-HST mergers at z similar to 1.5 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; galaxies: interactions; galaxies: starburst; galaxies: structure ID INTEGRAL FIELD SPECTROSCOPY; DISC GALAXY MERGERS; DARK ENERGY SURVEY; ULTRA-DEEP-FIELD; FORMING GALAXIES; MASSIVE GALAXIES; HIGH-REDSHIFT; FORMATION HISTORY; NEARBY GALAXIES; MAJOR MERGERS AB We present an analysis of the spatial distribution of star formation in a sample of 60 visually identified galaxy merger candidates at z > 1. Our sample, drawn from the 3D-HST survey, is flux limited and was selected to have high star formation rates based on fits of their broad-band, low spatial resolution spectral energy distributions. It includes plausible pre-merger (close pairs) and post-merger (single objects with tidal features) systems, with total stellar masses and star formation rates derived from multiwavelength photometry. Here we use near-infrared slitless spectra from 3D-HST which produce H alpha or [O III] emission line maps as proxies for star formation maps. This provides a first comprehensive high-resolution, empirical picture of where star formation occurred in galaxy mergers at the epoch of peak cosmic star formation rate. We find that detectable star formation can occur in one or both galaxy centres, or in tidal tails. The most common case (58 per cent) is that star formation is largely concentrated in a single, compact region, coincident with the centre of (one of) the merger components. No correlations between star formation morphology and redshift, total stellar mass or star formation rate are found. A restricted set of hydrodynamical merger simulations between similarly massive and gas-rich objects implies that star formation should be detectable in both merger components, when the gas fractions of the individual components are the same. This suggests that z similar to 1.5 mergers typically occur between galaxies whose gas fractions, masses and/or star formation rates are distinctly different from one another. C1 [Schmidt, Kasper B.; Rix, Hans-Walter; da Cunha, Elisabete; Maseda, Michael V.; van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Schmidt, Kasper B.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Brammer, Gabriel B.] European So Observ, Santiago 19, Chile. [Cox, Thomas J.] Carnegie Observ, Pasadena, CA 91101 USA. [van Dokkum, Pieter; Lundgren, Britt; Momcheva, Ivelina; Nelson, Erica J.; Skelton, Rosalind E.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Schreiber, Natascha M. Foerster] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Franx, Marijn; Fumagalli, Mattia] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Schmidt, KB (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM kschmidt@physics.ucsb.edu RI Skelton, Rosalind/S-1845-2016 OI Skelton, Rosalind/0000-0001-7393-3336 FU ERC grant HIGHZ [227749]; Marie Curie Initial Training Network ELIXIR of the European Commission [PITN-GA-2008-214227]; NASA [NAS5-26555] FX We acknowledge funding from ERC grant HIGHZ no. 227749. This work was funded in part by the Marie Curie Initial Training Network ELIXIR of the European Commission under contract PITN-GA-2008-214227. The work was mainly done while KBS was a member of the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg (IMPRS-HD), Germany. This work is based on observations taken by the 3D-HST Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 96 TC 9 Z9 9 U1 1 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 1 BP 285 EP 300 DI 10.1093/mnras/stt459 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600040 ER PT J AU Inayoshi, K Hosokawa, T Omukai, K AF Inayoshi, Kohei Hosokawa, Takashi Omukai, Kazuyuki TI Pulsational instability of supergiant protostars: do they grow supermassive by accretion? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: mass-loss; stars: oscillations; stars: Population III; stars: protostars; galaxies: nuclei; early Universe ID MAIN-SEQUENCE STARS; BLACK-HOLE FORMATION; MASSIVE PRIMORDIAL STARS; DARK-MATTER HALOES; DIRECT COLLAPSE; VIRIAL TEMPERATURES; VIBRATIONAL INSTABILITY; NONLINEAR PULSATIONS; EPSILON-MECHANISM; POPULATION III AB Supermassive stars (SMSs; M-* greater than or similar to 10(5) M-circle dot) and their remnant black holes are promising progenitors for supermassive black holes (SMBHs) observed in the early universe at z greater than or similar to 7. It has been postulated that SMSs form through very rapid mass accretion on to a protostar at a high rate exceeding 0.01 M-circle dot yr(-1). According to recent studies, such rapidly accreting protostars evolve into 'supergiant protostars', i.e. protostars consisting of a bloated envelope and a contracting core, similar to giant star. However, like massive stars as well as giant stars, both of which are known to be pulsationally unstable, supergiant protostars may also be unstable to launch strong pulsation-driven outflows. If this is the case, the stellar growth via accretion will be hindered by the mass-loss. We here study the pulsational stability of the supergiant protostars in the mass range M-* greater than or similar to 10(3) M-circle dot through the method of the linear perturbation analysis. We find that the supergiant protostars with M-* greater than or similar to 600 M-circle dot and very high accretion rate (M) over dot(acc) greater than or similar to 1.0 M-circle dot yr(-1) are unstable due to the kappa mechanism. The pulsation is excited in the He+ ionization layer in the envelope. Even under a conservative assumption that all the pulsation energy is converted into the kinetic energy of the outflows, the mass-loss rate is similar to 10(-) M-3(circle dot) yr(-1), which is lower than the accretion rate by more than two orders of magnitude. We thus conclude that the supergiant protostars should grow stably via rapid accretion at least in the mass range we studied. As long as the rapid accretion is maintained in the later stage, protostars will become SMSs, which eventually produce seeds for the high-z SMBHs. C1 [Inayoshi, Kohei; Omukai, Kazuyuki] Kyoto Univ, Grad Sch Sci, Dept Phys, Kyoto 6068502, Japan. [Hosokawa, Takashi] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Hosokawa, Takashi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Inayoshi, K (reprint author), Kyoto Univ, Grad Sch Sci, Dept Phys, Kyoto 6068502, Japan. EM inayoshi@tap.scphys.kyoto-u.ac.jp FU Ministry of Education, Culture, and Science of Japan [23.838, 2168407, 21244021] FX We would like to thank Takashi Nakamura for his continuous encouragement, Takafumi Sonoi and Kei Tanaka for fruitful discussions, and Shunsuke Katayama for improving the manuscript. This work is supported in part by the Grants-in-Aid by the Ministry of Education, Culture, and Science of Japan (23.838 KI; 2168407 and 21244021 KO). NR 55 TC 15 Z9 15 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 431 IS 4 BP 3036 EP 3044 DI 10.1093/mnras/stt362 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151RX UT WOS:000319479000007 ER PT J AU Cropper, M Hoekstra, H Kitching, T Massey, R Amiaux, J Miller, L Mellier, Y Rhodes, J Rowe, B Pires, S Saxton, C Scaramella, R AF Cropper, Mark Hoekstra, Henk Kitching, Thomas Massey, Richard Amiaux, Jerome Miller, Lance Mellier, Yannick Rhodes, Jason Rowe, Barnaby Pires, Sandrine Saxton, Curtis Scaramella, Roberto TI Defining a weak lensing experiment in space SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; methods: statistical; space vehicles: instruments; cosmological parameters; cosmology: observations ID POINT-SPREAD FUNCTION; GALAXY SHAPE MEASUREMENT; CHARGE-TRANSFER INEFFICIENCY; PIXEL-BASED CORRECTION; COSMIC SHEAR; ADVANCED CAMERA; DARK ENERGY; SYSTEMATIC-ERRORS; IMAGE-ANALYSIS; TELESCOPE AB This paper describes the definition of a typical next-generation space-based weak gravitational lensing experiment. We first adopt a set of top-level science requirements from the literature, based on the scale and depth of the galaxy sample, and the avoidance of systematic effects in the measurements which would bias the derived shear values. We then identify and categorize the contributing factors to the systematic effects, combining them with the correct weighting, in such a way as to fit within the top-level requirements. We present techniques which permit the performance to be evaluated and explore the limits at which the contributing factors can be managed. Besides the modelling biases resulting from the use of weighted moments, the main contributing factors are the reconstruction of the instrument point spread function, which is derived from the stellar images on the image, and the correction of the charge transfer inefficiency in the CCD detectors caused by radiation damage. C1 [Cropper, Mark; Kitching, Thomas; Saxton, Curtis] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Hoekstra, Henk] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kitching, Thomas; Massey, Richard] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Massey, Richard] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Amiaux, Jerome; Mellier, Yannick; Pires, Sandrine] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Miller, Lance] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Mellier, Yannick] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rhodes, Jason; Rowe, Barnaby] CALTECH, Pasadena, CA 91125 USA. [Rowe, Barnaby] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Scaramella, Roberto] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. RP Cropper, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM m.cropper@ucl.ac.uk RI Saxton, Curtis/A-6435-2013; OI Saxton, Curtis/0000-0002-5441-1978; Scaramella, Roberto/0000-0003-2229-193X; Rowe, Barnaby/0000-0002-7042-9174; Hoekstra, Henk/0000-0002-0641-3231 FU Netherlands Organization for Scientific Research through VIDI; Netherlands Research School for Astronomy (NOVA); Royal Astronomical Society; Royal Society; ERC International Reintegration Grants; European Research Council [240672]; JPL FX We thank Rene Laureijs, Pierre Ferruit, Tim Oosterbroek and Ludovic Duvet at ESA for their support. We also thank Elisabetta Semboloni for her comments on the paper. We acknowledge the referee who made some valuable suggestions which improved the accessibility of this paper. HH is supported by the Netherlands Organization for Scientific Research through VIDI grants and acknowledges support from the Netherlands Research School for Astronomy (NOVA). TDK was supported by a Royal Astronomical Society 2010 Fellowship and now by a Royal Society University Research Fellowship. RM is supported by a Royal Society University Research Fellowship. RM and HH also acknowledge support from ERC International Reintegration Grants. BR acknowledges support from European Research Council in the form of a Starting Grant with number 240672. JR was supported by JPL, run by Caltech under a contract for NASA. NR 76 TC 32 Z9 32 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 431 IS 4 BP 3103 EP 3126 DI 10.1093/mnras/stt384 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151RX UT WOS:000319479000011 ER PT J AU Otto, A Otto, FEL Boucher, O Church, J Hegerl, G Forster, PM Gillett, NP Gregory, J Johnson, GC Knutti, R Lewis, N Lohmann, U Marotzke, J Myhre, G Shindell, D Stevens, B Allen, MR AF Otto, Alexander Otto, Friederike E. L. Boucher, Olivier Church, John Hegerl, Gabi Forster, Piers M. Gillett, Nathan P. Gregory, Jonathan Johnson, Gregory C. Knutti, Reto Lewis, Nicholas Lohmann, Ulrike Marotzke, Jochem Myhre, Gunnar Shindell, Drew Stevens, Bjorn Allen, Myles R. TI Energy budget constraints on climate response SO NATURE GEOSCIENCE LA English DT Letter ID SENSITIVITY C1 [Otto, Alexander; Otto, Friederike E. L.; Allen, Myles R.] Univ Oxford, Environm Change Inst, Oxford OX1 3QY, England. [Boucher, Olivier] UPMC, CNRS, IPSL, Lab Meteorol Dynam, Paris, France. [Church, John] CSIRO Marine & Atmospher Res Hobart, Hobart, Tas 7000, Australia. [Hegerl, Gabi] Univ Edinburgh, Grant Inst, Edinburgh EH9 3JW, Midlothian, Scotland. [Forster, Piers M.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Gillett, Nathan P.] Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada. [Gregory, Jonathan] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. [Johnson, Gregory C.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Knutti, Reto; Lohmann, Ulrike] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. [Lewis, Nicholas] Walden, Bath BA2 6ED, Avon, England. [Marotzke, Jochem; Stevens, Bjorn] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Myhre, Gunnar] CICERO, N-0318 Oslo, Norway. [Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Allen, Myles R.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. RP Otto, A (reprint author), Univ Oxford, Environm Change Inst, S Parks Rd, Oxford OX1 3QY, England. EM alexander.otto@ouce.ox.ac.uk RI Church, John/A-1541-2012; Forster, Piers/F-9829-2010; Stevens, Bjorn/A-1757-2013; Johnson, Gregory/I-6559-2012; Knutti, Reto/B-8763-2008; Shindell, Drew/D-4636-2012; Myhre, Gunnar/A-3598-2008; Lohmann, Ulrike/B-6153-2009; Gregory, Jonathan/J-2939-2016 OI Church, John/0000-0002-7037-8194; Forster, Piers/0000-0002-6078-0171; Stevens, Bjorn/0000-0003-3795-0475; Johnson, Gregory/0000-0002-8023-4020; Knutti, Reto/0000-0001-8303-6700; Myhre, Gunnar/0000-0002-4309-476X; Lohmann, Ulrike/0000-0001-8885-3785; Gregory, Jonathan/0000-0003-1296-8644 FU Natural Environment Research Council [NE/E016189/1] NR 16 TC 107 Z9 107 U1 6 U2 103 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD JUN PY 2013 VL 6 IS 6 BP 415 EP 416 DI 10.1038/ngeo1836 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 154ET UT WOS:000319655200003 ER PT J AU Yoon, J Hunter, G Akbar, S Dutta, PK AF Yoon, Junro Hunter, Gary Akbar, Sheikh Dutta, Prabir K. TI Interface reaction and its effect on the performance of a CO2 gas sensor based on Li0.35La0.55TiO3 electrolyte and Li2CO3 sensing electrode SO SENSORS AND ACTUATORS B-CHEMICAL LA English DT Article DE CO2 sensor; Electrochemical device; Lithium lanthanum titanate; Electrode-electrolyte interface; Interface reaction; Lithium ion conductor ID SOLID REFERENCE ELECTRODE; LITHIUM LANTHANUM TITANATES; ELECTROCHEMICAL CO2; POTENTIOMETRIC SENSOR; IONIC-CONDUCTIVITY; TEMPERATURE; STABILITY; NASICON; OXIDE; LA0.67-XLI3XTIO3 AB A new potentiometric CO2 gas sensor using lithium-lanthanum-titanate (Li0.35La0.55TiO3, LLTO) electrolyte, Li2CO3 sensing electrode, and Li2TiO3 + TiO2 reference electrode was investigated. The microstructure and electrical properties of the optimized solid electrolyte were examined and the measured conductivity values were found consistent with those reported in literature. The performance of the sensor depended both on the fabrication temperature and the sensor operation temperature. Sensors with the sensing electrode fabricated above 500 degrees C performed poorly. For sensing electrodes fabricated at 500 degrees C, as the sensing temperature increased from 300 to 450 degrees C, the performance of the sensor improved (near Nernstian response), but above 450 degrees C, the sensor degraded. The proposed hypothesis for the degradation beyond 450 degrees C is that at low levels of CO2 (ppb in the background), Li2CO3 reacts with LLTO resulting in insertion of Li+ into LLTO that causes changes in the electrical properties of the electrolyte. Poor performance of sensors fabricated at 700 degrees C was due to formation of a new phase, LaLi1/3Ti2/3O3. Thermodynamic calculations combined with X-ray diffraction of the reaction products are used to support the hypothesis. Introduction of high concentrations of CO2 (similar to 99.99%) during sensor fabrication (650 degrees C) eliminated the reaction between Li2CO3 and LLTO, and also facilitated the bonding between the electrode and the electrolyte. As for long-term device performance, it is shown that the sensor can measure changes in CO2 concentrations reproducibly below temperatures of 450 degrees C, as long as it is operated in conditions where there is a background of CO2, such as in ambient atmosphere or combustion environments. The sensor exhibits minimal interference toward oxygen, but significant interference to humidity. (C) 2013 Elsevier B.V. All rights reserved. C1 [Yoon, Junro; Akbar, Sheikh; Dutta, Prabir K.] Ohio State Univ, Ctr Ind Sensors & Measurements, Columbus, OH 43210 USA. [Yoon, Junro; Akbar, Sheikh] Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA. [Hunter, Gary] NASA, Glenn Res Ctr, Cleveland, OH USA. [Dutta, Prabir K.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. RP Akbar, S (reprint author), Ohio State Univ, Ctr Ind Sensors & Measurements, 2041 Coll Rd, Columbus, OH 43210 USA. EM akbar@matsceng.ohio-state.edu; dutta.1@osu.edu RI Akbar, Sheikh/J-6170-2013 OI Akbar, Sheikh/0000-0003-3567-274X FU NASA FX We acknowledge funding from NASA for this research. NR 53 TC 7 Z9 7 U1 3 U2 53 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-4005 J9 SENSOR ACTUAT B-CHEM JI Sens. Actuator B-Chem. PD JUN PY 2013 VL 182 BP 95 EP 103 DI 10.1016/j.snb.2013.02.104 PG 9 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA 151VP UT WOS:000319488800014 ER PT J AU Lintott, CJ Schwamb, ME Barclay, T Sharzer, C Fischer, DA Brewer, J Giguere, M Lynn, S Parrish, M Batalha, N Bryson, S Jenkins, J Ragozzine, D Rowe, JF Schwainski, K Gagliano, R Gilardi, J Jek, KJ Paakkonen, JP Smits, T AF Lintott, Chris J. Schwamb, Megan E. Barclay, Thomas Sharzer, Charlie Fischer, Debra A. Brewer, John Giguere, Matthew Lynn, Stuart Parrish, Michael Batalha, Natalie Bryson, Steve Jenkins, Jon Ragozzine, Darin Rowe, Jason F. Schwainski, Kevin Gagliano, Robert Gilardi, Joe Jek, Kian J. Paeaekkoenen, Jari-Pekka Smits, Tjapko TI PLANET HUNTERS: NEW KEPLER PLANET CANDIDATES FROM ANALYSIS OF QUARTER 2 SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites: detection; planets and satellites: individual (KIC 4552729b, KIC 10005758b, KIC 10005758c) ID GALAXY ZOO; SYSTEMS; STELLAR AB We present new planet candidates identified in NASA Kepler Quarter 2 public release data by volunteers engaged in the Planet Hunters citizen science project. The two candidates presented here survive checks for false positives, including examination of the pixel offset to constrain the possibility of a background eclipsing binary. The orbital periods of the planet candidates are 97.46 days (KIC 4552729) and 284.03 (KIC 10005758) days and the modeled planet radii are 5.3 and 3.8R(circle plus). The latter star has an additional known planet candidate with a radius of 5.05R(circle plus) and a period of 134.49 days, which was detected by the Kepler pipeline. The discovery of these candidates illustrates the value of massively distributed volunteer review of the Kepler database to recover candidates which were otherwise uncataloged. C1 [Lintott, Chris J.] Oxford Astrophys, Oxford OX1 3RH, England. [Lintott, Chris J.; Lynn, Stuart; Parrish, Michael] Adler Planetarium, Chicago, IL 60605 USA. [Schwamb, Megan E.; Schwainski, Kevin] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Schwamb, Megan E.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Barclay, Thomas; Batalha, Natalie; Bryson, Steve; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Sharzer, Charlie; Fischer, Debra A.; Brewer, John; Giguere, Matthew] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Jenkins, Jon] SETI Inst, Mountain View, CA 94043 USA. [Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lintott, CJ (reprint author), Oxford Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM cjl@astro.ox.ac.uk OI Brewer, John/0000-0002-9873-1471; Schwamb, Megan/0000-0003-4365-1455; Fischer, Debra/0000-0003-2221-0861 FU Yale University; NASA [10-OUTRCH.210-0001, NAS5-26555]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-100325]; Leverhulme Trust; National Science Foundation [DRL-0941610]; National Aeronautics and Space Administration; NASA Office of Space Science [NNX09AF08G] FX D.F. acknowledges funding support from Yale University and support from the NASA Supplemental Outreach Award, 10-OUTRCH.210-0001. M.E.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-100325. The Zooniverse is supported by The Leverhulme Trust. The Talk system used by Planet Hunters was built during work supported by the National Science Foundation under grant No. DRL-0941610. We gratefully acknowledge the dedication and achievements of Kepler Science Team and all those who contributed to the success of the mission. We acknowledge use of public release data served by the NASA/IPAC/NExScI Star and Exoplanet Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System Bibliographic Services. This paper includes data collected by the Kepler spacecraft, and we gratefully acknowledge the entire Kepler mission team's efforts in obtaining and providing the light curves used in this analysis. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The publicly released Kepler light curves were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 26 TC 10 Z9 10 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2013 VL 145 IS 6 AR 151 DI 10.1088/0004-6256/145/6/151 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 147LC UT WOS:000319167400008 ER PT J AU Lang, C Doostan, A Maute, K AF Lang, Christapher Doostan, Alireza Maute, Kurt TI Extended stochastic FEM for diffusion problems with uncertain material interfaces SO COMPUTATIONAL MECHANICS LA English DT Article DE X-SFEM; Polynomial chaos; Level set method; Uncertainty analysis; Enrichment ID FINITE-ELEMENT-METHOD; PARTIAL-DIFFERENTIAL-EQUATIONS; LEVEL SET METHOD; POLYNOMIAL CHAOS; COMPOSITE-MATERIALS; RANDOM DOMAINS; CRACK-GROWTH; PROPAGATION; INCLUSIONS; SIMULATION AB This paper is concerned with the prediction of heat transfer in composite materials with uncertain inclusion geometry. To numerically solve the governing equation, which is defined on a random domain, an approach based on the combination of the Extended finite element method (X-FEM) and the spectral stochastic finite element method is studied. Two challenges of the extended stochastic finite element method (X-SFEM) are choosing an enrichment function and numerical integration over the probability domain. An enrichment function, which is based on knowledge of the interface location, captures the C-0-continuous solution in the spatial and probability domains without a conforming mesh. Standard enrichment functions and enrichment functions tailored to X-SFEM are analyzed and compared, and the basic elements of a successful enrichment function are identified. We introduce a partition approach for accurate integration over the probability domain. The X-FEM solution is studied as a function of the parameters describing the inclusion geometry and the different enrichment functions. The efficiency and accuracy of a spectral polynomial chaos expansion and a finite element approximation in the probability domain are compared. Numerical examples of a two-dimensional heat conduction problem with a random inclusion show the spectral PC approximation with a suitable choice of enrichment function is as accurate and more efficient than the finite element approach. Though focused on heat transfer in composite materials, the techniques and observations in this paper are also applicable to other types of problems with uncertain geometry. C1 [Lang, Christapher] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23665 USA. [Doostan, Alireza; Maute, Kurt] Univ Colorado, Boulder, CO 80309 USA. RP Doostan, A (reprint author), Univ Colorado, Boulder, CO 80309 USA. EM alireza.doostan@colorado.edu FU NASA Fundamental Aeronautics Program; Department of Energy [DE-SC0006402]; National Science Foundation [EFRI-1038305] FX The first author acknowledges the support of the NASA Fundamental Aeronautics Program, and the second author acknowledges the support of the Department of Energy under grant DE-SC0006402. The third author acknowledges the support of the National Science Foundation under grant EFRI-1038305. The opinions and conclusions presented are those of the authors and do not necessarily reflect the views of the sponsoring organizations. NR 40 TC 7 Z9 7 U1 0 U2 15 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0178-7675 J9 COMPUT MECH JI Comput. Mech. PD JUN PY 2013 VL 51 IS 6 BP 1031 EP 1049 DI 10.1007/s00466-012-0785-8 PG 19 WC Mathematics, Interdisciplinary Applications; Mechanics SC Mathematics; Mechanics GA 149UI UT WOS:000319346500013 ER PT J AU Atteia, GE Collins, MJ AF Atteia, G. E. Collins, Michael J. TI On the use of compact polarimetry SAR for ship detection SO ISPRS JOURNAL OF PHOTOGRAMMETRY AND REMOTE SENSING LA English DT Article DE Ship detection; Polarimetry; Compact polarimetry; Synthetic aperture radar ID SYNTHETIC-APERTURE RADAR; POL SAR; CLASSIFICATION; ARCHITECTURE; PERFORMANCE AB Quad-pol data are generally acknowledged as providing the highest performance in ship detection applications using SAR data. Yet quad-pol data have half the swath width of single and dual-pol data and are thus less useful for maritime surveillance, where wide area coverage is crucial. Compact polarimetry (CP) has been proposed as a compromise between swath width and polarization information. The circular-transmit-linear-receive (CTLR) CP data have certain engineering advantages over other CP configurations. CF data may be used to reconstruct a reduced quad-pol covariance matrix (termed pseudo-quad, or PQ data) and the potential of these data in terrestrial applications has recently been demonstrated. We present some of the first results on the use of CTLR data and reconstructed quad-pol data for ship detection. We use Radarsat-2 fine-quad (FQ) data to examine 76 ships over a range of incidence angles and ship orientations at low to moderate wind speeds. We examined the ship detection performance of full quad-pol and full-PQ data; several dual-pol configurations suggested in the literature, HV and PQ HV and the raw CTLR data. We find that the ship detection performance of the PQHV data is the strongest of all the detectors we examined, with performance that was comparable to quad-pol data. Other strong performers were HV and CTLR data. (C) 2013 International Society for Photogrammetry and Remote Sensing, Inc. (ISPRS) Published by Elsevier B.V. All rights reserved. C1 [Atteia, G. E.; Collins, Michael J.] Univ Calgary, Dept Geomat Engn, Calgary, AB T2N 1N4, Canada. [Collins, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Collins, MJ (reprint author), Univ Calgary, Dept Geomat Engn, Calgary, AB T2N 1N4, Canada. EM mjcollin@ucalgary.ca RI chen, zhu/K-5923-2013 FU Defence Research and Development Canada; Natural Science and Engineering Research Council (NSERC) of Canada FX Paris Vachon of Defence Research and Development Canada provided both funding and data. Chen Liu, also of DRDC, helped us implement the LRT. We also acknowledge Francois Charbonneau, of the Canada Centre for Remote Sensing, for leading the Canadian working group on compact polarimetry. We further acknowledge funding support from Natural Science and Engineering Research Council (NSERC) of Canada. NR 46 TC 18 Z9 21 U1 0 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0924-2716 J9 ISPRS J PHOTOGRAMM JI ISPRS-J. Photogramm. Remote Sens. PD JUN PY 2013 VL 80 BP 1 EP 9 DI 10.1016/j.isprsjprs.2013.01.009 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 148KI UT WOS:000319243100001 ER PT J AU Orwoll, ES Adler, RA Amin, S Binkley, N Lewiecki, EM Petak, SM Shapses, SA Sinaki, M Watts, NB Sibonga, JD AF Orwoll, Eric S. Adler, Robert A. Amin, Shreyasee Binkley, Neil Lewiecki, E. Michael Petak, Steven M. Shapses, Sue A. Sinaki, Mehrsheed Watts, Nelson B. Sibonga, Jean D. TI Skeletal health in long-duration astronauts: Nature, assessment, and management recommendations from the NASA bone summit SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Review DE SPACEFLIGHT; OSTEOPOROSIS; QCT; FINITE ELEMENT MODELING; DXA; FRACTURE; MICROGRAVITY ID PROXIMAL FEMORAL STRENGTH; FINITE-ELEMENT-ANALYSIS; BED-REST; SPACE-FLIGHT; HIP FRACTURE; MINERAL DENSITY; CANCELLOUS BONE; SPACEFLIGHT; MEN; WEIGHTLESSNESS AB Concern about the risk of bone loss in astronauts as a result of prolonged exposure to microgravity prompted the National Aeronautics and Space Administration to convene a Bone Summit with a panel of experts at the Johnson Space Center to review the medical data and research evidence from astronauts who have had prolonged exposure to spaceflight. Data were reviewed from 35 astronauts who had served on spaceflight missions lasting between 120 and 180 days with attention focused on astronauts who (1) were repeat fliers on long-duration missions, (2) were users of an advanced resistive exercise device (ARED), (3) were scanned by quantitative computed tomography (QCT) at the hip, (4) had hip bone strength estimated by finite element modeling, or (5) had lost >10% of areal bone mineral density (aBMD) at the hip or lumbar spine as measured by dual-energy X-ray absorptiometry (DXA). Because of the limitations of DXA in describing the effects of spaceflight on bone strength, the panel recommended that the U.S. space program use QCT and finite element modeling to further study the unique effects of spaceflight (and recovery) on bone health in order to better inform clinical decisions. C1 [Orwoll, Eric S.] Oregon Hlth & Sci Univ, Bone & Mineral Unit, Portland, OR 97201 USA. [Adler, Robert A.] McGuire Vet Affairs Med Ctr, Dept Endocrinol, Richmond, VA USA. [Adler, Robert A.] Virginia Commonwealth Univ, Sch Med, Richmond, VA USA. [Amin, Shreyasee] Mayo Clin, Div Rheumatol, Rochester, MN USA. [Binkley, Neil] Univ Wisconsin, Osteoporosis Clin Ctr, Madison, WI USA. [Binkley, Neil] Univ Wisconsin, Res Program, Madison, WI USA. [Lewiecki, E. Michael] New Mexico Clin Res & Osteoporosis Ctr, Albuquerque, NM USA. [Petak, Steven M.] Texas Inst Reprod Med & Endocrinol, Houston, TX USA. [Shapses, Sue A.] Rutgers State Univ, Dept Nutr Sci, New Brunswick, NJ 08903 USA. [Sinaki, Mehrsheed] Mayo Clin, Dept Phys Med & Rehabil, Rochester, MN USA. [Watts, Nelson B.] Mercy Hlth Osteoporosis Serv, Cincinnati, OH USA. [Watts, Nelson B.] Mercy Bone Hlth Serv, Cincinnati, OH USA. [Sibonga, Jean D.] NASA, Human Hlth & Performance Directorate, Johnson Space Ctr, Houston, TX 77058 USA. RP Sibonga, JD (reprint author), NASA, Bone & Mineral Lab SK 272, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM Jean.sibonga-1@nasa.gov OI Orwoll, Eric/0000-0002-8520-7355 FU Human Adaptation and Countermeasures Division at NASA Johnson Space Center FX Appreciation is extended to Dr. Angelo A. Licata (Cleveland Clinic, Center for Space Medicine) and Dr. S. V. Reddy (Medical University of South Carolina) for their thoughtful review of this manuscript and to Dr. Jane Krauhs and Dr. Kathleen McMonigal, MD (both of Johnson Space Center) for their editorial assistance. In addition, authors wish to acknowledge the contributions of Dr. Scott M. Smith, Dr. Sara R. Zwart, Dr. Andrea M. Hanson, Dr. Harlan Evans, Ms. Elisabeth R. Spector, and Ms. Adriana Babiak-Vazquez (all of Johnson Space Center), Dr. Adrian D. LeBlanc (Universities Space Research Association), Dr. Thomas F. Lang (University of California at San Francisco), and Dr. Joyce H. Keyak (University of California at Irvine) for the presentations of astronaut data in this review. The Bone Summit activity was funded by Human Adaptation and Countermeasures Division at NASA Johnson Space Center. NR 38 TC 27 Z9 31 U1 1 U2 36 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0884-0431 J9 J BONE MINER RES JI J. Bone Miner. Res. PD JUN PY 2013 VL 28 IS 6 BP 1243 EP 1255 DI 10.1002/jbmr.1948 PG 13 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 149VS UT WOS:000319350100001 PM 23553962 ER PT J AU Plante, I Devroye, L Cucinotta, FA AF Plante, Ianik Devroye, Luc Cucinotta, Francis A. TI Random sampling of the Green's Functions for reversible reactions with an intermediate state SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Computer simulations; Monte-Carlo simulations; Single molecule reaction kinetics; Biophysical mechanisms of interaction ID MONTE-CARLO-SIMULATION; ONE-DIMENSION; LIQUID WATER; GEMINATE RECOMBINATION; BIMOLECULAR REACTIONS; FRICKE DOSIMETER; DIFFUSION; RADIOLYSIS; RADIATION; KINETICS AB Exact random variate generators were developed to sample Green's functions used in Brownian Dynamics (BD) algorithms for the simulations of chemical systems. These algorithms, which use less than a kilobyte of memory, provide a useful alternative to the table look-up method that has been used in similar work. The cases that are studied with this approach are (1) diffusion-influenced reactions; (2) reversible diffusion-influenced reactions and (3) reactions with an intermediate state such as enzymatic catalysis. The results are validated by comparison with those obtained by the Independent Reaction Times (IRT) method. This work is part of our effort in developing models to understand the role of radiation chemistry in the radiation effects on human body and may eventually be included in event-based models of space radiation risk. (C) 2013 Elsevier Inc. All rights reserved. C1 [Plante, Ianik] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Devroye, Luc] McGill Univ, Sch Comp Sci, Montreal, PQ H3A 0E9, Canada. RP Plante, I (reprint author), NASA, Lyndon B Johnson Space Ctr, Bldg 37,2101 NASA Pkwy, Houston, TX 77058 USA. EM ianik.plante-1@nasa.gov; lucdevroye@gmail.com; Francis.A.Cucinotta@nasa.gov FU NASA Space Radiation Risk Assessment Project FX This work was supported by the NASA Space Radiation Risk Assessment Project. We would also like to thank Drs. Noam Agmon and Dr. Soohyung Park for useful correspondence. NR 34 TC 4 Z9 4 U1 0 U2 6 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 JUN 1 PY 2013 VL 242 BP 531 EP 543 DI 10.1016/j.jcp.2013.02.001 PG 13 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 145WK UT WOS:000319049800026 ER PT J AU Breuner, CW Sprague, RS Patterson, SH Woods, HA AF Breuner, Creagh W. Sprague, Rachel S. Patterson, Stephen H. Woods, H. Arthur TI Environment, behavior and physiology: do birds use barometric pressure to predict storms? SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE activity; corticosterone; environmental cues; inclement weather; metabolic rate; stress ID WHITE-CROWNED SPARROWS; FOOD-INTAKE; CORTICOSTERONE RESPONSES; ADRENOCORTICAL-RESPONSE; ATMOSPHERIC-PRESSURE; AMBIENT-TEMPERATURE; PARATYMPANIC ORGAN; PASSERINE BIRDS; SIERRA-NEVADA; WEATHER AB Severe storms can pose a grave challenge to the temperature and energy homeostasis of small endothermic vertebrates. Storms are accompanied by lower temperatures and wind, increasing metabolic expenditure, and can inhibit foraging, thereby limiting energy intake. To avoid these potential problems, most endotherms have mechanisms for offsetting the energetic risks posed by storms. One possibility is to use cues to predict oncoming storms and to alter physiology and behavior in ways that make survival more likely. Barometric pressure declines predictably before inclement weather, and several lines of evidence indicate that animals alter behavior based on changes in ambient pressure. Here we examined the effects of declining barometric pressure on physiology and behavior in the white-crowned sparrow, Zonotrichia leucophrys. Using field data from a long-term study, we first evaluated the relationship between barometric pressure, storms and stress physiology in free-living white-crowned sparrows. We then manipulated barometric pressure experimentally in the laboratory and determined how it affects activity, food intake, metabolic rates and stress physiology. The field data showed declining barometric pressure in the 12-24 h preceding snowstorms, but we found no relationship between barometric pressure and stress physiology. The laboratory study showed that declining barometric pressure stimulated food intake, but had no effect on metabolic rate or stress physiology. These data suggest that white-crowned sparrows can sense and respond to declining barometric pressure, and we propose that such an ability may be common in wild vertebrates, especially small ones for whom individual storms can be life-threatening events. C1 [Breuner, Creagh W.; Sprague, Rachel S.] Univ Montana, Wildlife Biol Program, Missoula, MT 59812 USA. [Breuner, Creagh W.; Patterson, Stephen H.; Woods, H. Arthur] Univ Montana, Missoula, MT 59812 USA. [Sprague, Rachel S.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Reg Off, Honolulu, HI 96814 USA. RP Breuner, CW (reprint author), Univ Montana, Wildlife Biol Program, 32 Campus Dr, Missoula, MT 59812 USA. EM creagh.breuner@umontana.edu FU National Science Foundation [IBN 0236536, IOS 0747361] FX This work was supported by the National Science Foundation [IBN 0236536, IOS 0747361 to C.W.B.]. NR 57 TC 8 Z9 10 U1 3 U2 64 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 JUN PY 2013 VL 216 IS 11 BP 1982 EP 1990 DI 10.1242/jeb.081067 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 146UG UT WOS:000319117400013 PM 23678098 ER PT J AU Wu, K Choudhury, D Matsumoto, H AF Wu, Ke Choudhury, Debabani Matsumoto, Hiroshi TI Wireless Power Transmission, Technology, and Applications SO PROCEEDINGS OF THE IEEE LA English DT Editorial Material C1 [Wu, Ke] Southeast Univ, Boston, MA USA. [Wu, Ke] Univ Montreal, Ecole Polytech, Montreal, PQ, Canada. [Wu, Ke] Nanjing Univ Sci & Technol, Nanjing, Jiangsu, Peoples R China. [Wu, Ke] Nanjing Univ Post Telecommun, Nanjing, Jiangsu, Peoples R China. [Wu, Ke] City Univ Hong Kong, Hong Kong, Hong Kong, Peoples R China. [Choudhury, Debabani] Millitech Corp, Northampton, MA USA. [Choudhury, Debabani] NASA, Jet Prop Lab, Washington, DC USA. [Matsumoto, Hiroshi] Kyoto Univ, Kyoto 6068501, Japan. [Matsumoto, Hiroshi] Kyoto Univ, Fac Engn, Kyoto 6068501, Japan. [Matsumoto, Hiroshi] Kyoto Univ, Radio Sci Ctr Space & Atmosphere, Kyoto 6068501, Japan. RP Wu, K (reprint author), Southeast Univ, Boston, MA USA. NR 0 TC 20 Z9 22 U1 0 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9219 J9 P IEEE JI Proc. IEEE PD JUN PY 2013 VL 101 IS 6 SI SI BP 1271 EP 1275 DI 10.1109/JPROC.2013.2257590 PG 5 WC Engineering, Electrical & Electronic SC Engineering GA 147DY UT WOS:000319147000002 ER PT J AU Xu, TB Siochi, EJ Kang, JH Zuo, L Zhou, WL Tang, XD Jiang, XN AF Xu, Tian-Bing Siochi, Emilie J. Kang, Jin Ho Zuo, Lei Zhou, Wanlu Tang, Xiudong Jiang, Xiaoning TI Energy harvesting using a PZT ceramic multilayer stack SO SMART MATERIALS AND STRUCTURES LA English DT Article ID AIRPLANE FUSELAGE STRUCTURE; VIBRATION MEASUREMENTS; STRESS; CIRCUIT; CAPACITANCE; TRANSDUCER; EXCITATION; DEPENDENCE; CRYSTALS; CYMBAL AB In this paper, the interdisciplinary energy harvesting issues on piezoelectric energy harvesting were investigated using a '33' mode (mechanical stress and/or electric field are in parallel to the polarization direction) lead zirconate titanate multilayer piezoelectric stack (PZT-Stack). Key energy harvesting characteristics including the generated electrical energy/power in the PZT-Stack, the mechanical to electrical energy conversion efficiency, the power delivered from the PZT-Stack to a resistive load, the electrical charge/energy transferred from the PZT-Stack to a super-capacitor were systematically addressed. Theoretical models for power generation and delivery to a resistive load were proposed and experimentally affirmed. In a quasi-static regime, 70% generated electrical powers were delivered to matched resistive loads. A 35% mechanical to electrical energy conversion efficiency, which is more than 4 times higher than other reports, for the PZT-Stack had been obtained. The generated electrical power and power density were significantly higher than those from a similar weight and size cantilever-type piezoelectric harvester in both resonance and off-resonance modes. In addition, our study indicated that the capacitance and piezoelectric coefficient of the PZT-Stack were strongly dependent on the dynamic stress. C1 [Xu, Tian-Bing; Kang, Jin Ho] Natl Inst Aerosp, Hampton, VA 23666 USA. [Siochi, Emilie J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Zuo, Lei; Zhou, Wanlu; Tang, Xiudong] SUNY Stony Brook, Dept Mech Engn, Stony Brook, NY 11794 USA. [Jiang, Xiaoning] N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA. RP Xu, TB (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM tbxu@nianet.org RI Jiang, Xiaoning/E-6619-2011; Zuo, Lei/B-3122-2017 OI Jiang, Xiaoning/0000-0003-3605-3801; NR 51 TC 27 Z9 27 U1 6 U2 74 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 EI 1361-665X J9 SMART MATER STRUCT JI Smart Mater. Struct. PD JUN PY 2013 VL 22 IS 6 AR 065015 DI 10.1088/0964-1726/22/6/065015 PG 15 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA 147VH UT WOS:000319195500016 ER PT J AU Yu, LY Leckey, CAC Tian, ZH AF Yu, Lingyu Leckey, Cara A. C. Tian, Zhenhua TI Study on crack scattering in aluminum plates with Lamb wave frequency-wavenumber analysis SO SMART MATERIALS AND STRUCTURES LA English DT Article ID FINITE INTEGRATION TECHNIQUE; LASER AB The multimodal characteristic of Lamb waves makes the interpretation of Lamb wave signals difficult in either the time or frequency domain. In this work, we present our study of Lamb wave propagation characterization and crack scattering using frequency-wavenumber analysis. The aim is to investigate three dimensional (3D) Lamb wave behavior in the presence of crack damage via the application of frequency-wavenumber analysis. The analysis techniques are demonstrated using simulation examples of an aluminum plate with a through-thickness crack. Both in-plane and out-of-plane components are acquired through a 3D elastodynamic finite integration technique (EFIT), while the out-of-plane component is also experimentally obtained using a scanning laser Doppler vibrometer for verification purposes. The time-space wavefield is then transformed to the frequency-wavenumber domain by a two dimensional (2D) Fourier transform and the out-of-plane EFIT results are compared to experimental measurements. The experimental and simulated results are found to be in close agreement. The frequency-wavenumber representation of in-plane and out-of-plane components shows clear distinction among various Lamb wave modes that are present. However, spatial information is lost during this 2D transformation. A short space 2D Fourier transform is therefore adopted to obtain the frequency-wavenumber spectra at various spatial locations, resulting in a space-frequency-wavenumber representation of the signal. The space-frequency-wavenumber analysis has shown its potential for indicating crack presence. C1 [Yu, Lingyu; Tian, Zhenhua] Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA. [Leckey, Cara A. C.] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23665 USA. RP Yu, LY (reprint author), Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA. EM yu3@mailbox.sc.edu RI Tian, Zhenhua/I-6687-2015 OI Tian, Zhenhua/0000-0002-1903-5604 FU US Nuclear Regulatory Commission [NRC-04-10-155] FX Part of this work is conducted through the non-reimbursement space act umbrella agreement SAA1-1181 between South Carolina Research Foundation (SCRF) and the National Aeronautics and Space Administration (NASA) Langley research center. Part of this work is supported by the US Nuclear Regulatory Commission award NRC-04-10-155. NR 32 TC 22 Z9 23 U1 2 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 EI 1361-665X J9 SMART MATER STRUCT JI Smart Mater. Struct. PD JUN PY 2013 VL 22 IS 6 AR 065019 DI 10.1088/0964-1726/22/6/065019 PG 12 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA 147VH UT WOS:000319195500020 ER PT J AU Branscomb, E Russell, MJ AF Branscomb, Elbert Russell, Michael J. TI Turnstiles and bifurcators: The disequilibrium converting engines that put metabolism on the road (vol 1827, pg 62, 2013) SO BIOCHIMICA ET BIOPHYSICA ACTA-BIOENERGETICS LA English DT Correction C1 [Branscomb, Elbert] UIUC, Inst Genom Biol, Champaign, IL USA. [Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Branscomb, E (reprint author), UIUC, Inst Genom Biol, Champaign, IL USA. EM brnscmb@illinois.edu NR 1 TC 0 Z9 0 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0005-2728 J9 BBA-BIOENERGETICS JI Biochim. Biophys. Acta-Bioenerg. PD JUN PY 2013 VL 1827 IS 6 BP 806 EP 806 DI 10.1016/j.bbabio.2013.02.017 PG 1 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA 146KG UT WOS:000319089400014 ER PT J AU Casner, SM Geven, RW Williams, KT AF Casner, Stephen M. Geven, Richard W. Williams, Kent T. TI The Effectiveness of Airline Pilot Training for Abnormal Events SO HUMAN FACTORS LA English DT Article DE abnormal events; generalizability; effectiveness; rote learning; training; pilots AB Objective: To evaluate the effectiveness of airline pilot training for abnormal in-flight events. Background: Numerous accident reports describe situations in which pilots responded to abnormal events in ways that were different from what they had practiced many times before. One explanation for these missteps is that training and testing for these skills have become a highly predictable routine for pilots who arrive to the training environment well aware of what to expect. Under these circumstances, pilots get plentiful practice in responding to abnormal events but may get little practice in recognizing them and deciding which responses to offer. Method: We presented 18 airline pilots with three abnormal events that are required during periodic training and testing. Pilots were presented with each event under the familiar circumstances used during training and also under less predictable circumstances as they might occur during flight. Results: When presented in the routine ways seen during training, pilots gave appropriate responses and showed little variability. However, when the abnormal events were presented unexpectedly, pilots' responses were less appropriate and showed great variability from pilot to pilot. Conclusion: The results suggest that the training and testing practices used in airline training may result in rote-memorized skills that are specific to the training situation and that offer modest generalizability to other situations. We recommend a more complete treatment of abnormal events that allows pilots to practice recognizing the event and choosing and recalling the appropriate response. Application: The results will aid the improvement of existing airline training practices. C1 [Casner, Stephen M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Geven, Richard W.; Williams, Kent T.] San Jose State Univ, Res Fdn, San Jose, CA 95192 USA. RP Casner, SM (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA. EM stephen.casner@nasa.gov NR 23 TC 6 Z9 6 U1 0 U2 12 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0018-7208 J9 HUM FACTORS JI Hum. Factors PD JUN PY 2013 VL 55 IS 3 BP 477 EP 485 DI 10.1177/0018720812466893 PG 9 WC Behavioral Sciences; Engineering, Industrial; Ergonomics; Psychology, Applied; Psychology SC Behavioral Sciences; Engineering; Psychology GA 144MF UT WOS:000318942900001 PM 23829023 ER PT J AU Bandler, SR Adams, JS Bailey, CN Busch, SE Chervenak, JA Eckart, ME Ewin, AE Finkbeiner, FM Kelley, RL Kelly, DP Kilbourne, CA Porst, JP Porter, FS Sadleir, JE Smith, SJ Wassell, EJ AF Bandler, Simon R. Adams, Joseph S. Bailey, Catherine N. Busch, Sarah E. Chervenak, James A. Eckart, Megan E. Ewin, Audrey E. Finkbeiner, Fred M. Kelley, Richard L. Kelly, Daniel P. Kilbourne, Caroline A. Porst, Jan-Patrick Porter, Frederick S. Sadleir, John E. Smith, Stephen J. Wassell, Edward J. TI Advances in Small Pixel TES-Based X-Ray Microcalorimeter Arrays for Solar Physics and Astrophysics SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Arrays; low temperature detectors; microcalorimeters; transition-edge sensors (TES); X-ray spectroscopy ID TRANSITION-EDGE SENSORS; LINES; RESOLUTION; NOISE AB We are developing small-pixel transition-edge sensor microcalorimeters for solar physics and astrophysics applications. These large format close-packed arrays are fabricated on solid silicon substrates and are designed to have high energy resolution, and also accommodate count-rates of up to a few hundred counts per second per pixel for X-ray photon energies up to similar to 8 keV. We have fabricated kilo-pixel versions that utilize narrow-line planar and stripline wiring. These arrays have a low superconducting transition temperature, which results in a low heat capacity and low thermal conductance to the heat sink. We present measurements of the performance of pixels with single 65-mu m absorbers on a 75-mu m pitch. With individual single pixels of this type, we have achieved a full-width at half-maximum energy resolution of 0.9 eV with 1.5 keV Al K X-rays, to our knowledge the first X-ray microcalorimeter with sub-eV energy resolution. We will discuss the properties of these arrays and their application to new solar and astrophysics mission concepts. C1 [Bandler, Simon R.; Adams, Joseph S.; Bailey, Catherine N.; Busch, Sarah E.; Chervenak, James A.; Eckart, Megan E.; Ewin, Audrey E.; Finkbeiner, Fred M.; Kelley, Richard L.; Kelly, Daniel P.; Kilbourne, Caroline A.; Porst, Jan-Patrick; Porter, Frederick S.; Sadleir, John E.; Smith, Stephen J.; Wassell, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bandler, Simon R.; Adams, Joseph S.; Eckart, Megan E.; Smith, Stephen J.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Porst, Jan-Patrick] Brown Univ, Providence, RI 02912 USA. [Kelly, Daniel P.; Wassell, Edward J.] MEI Technol Inc, Seabrook, MD 20706 USA. RP Bandler, SR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jp.porst@nasa.gov RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Porter, Frederick/D-3501-2012; Bailey, Catherine/C-6107-2009 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Porter, Frederick/0000-0002-6374-1119; FU NASA (Office of Space Science from ROSES) [NNX11AB47G] FX This work was supported by NASA (Office of Space Science, Contract NNX11AB47G from ROSES 2009). NR 19 TC 15 Z9 15 U1 2 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2100705 DI 10.1109/TASC.2013.2238752 PN 1 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100045 ER PT J AU Crowe, EJ Bennett, CL Chuss, DT Denis, KL Eimer, J Lourie, N Marriage, T Moseley, SH Rostem, K Stevenson, TR Towner, D U-yen, K Wollack, EJ AF Crowe, Erik J. Bennett, Charles L. Chuss, David T. Denis, Kevin L. Eimer, Joseph Lourie, Nathan Marriage, Tobias Moseley, Samuel H. Rostem, Karwan Stevenson, Thomas R. Towner, Deborah U-yen, Kongpop Wollack, Edward J. TI Fabrication of a Silicon Backshort Assembly for Waveguide-Coupled Superconducting Detectors SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Deep reactive ion etching; superconducting microstrip; surface roughness; transition edge sensors; wafer bonding ID MICROWAVE BACKGROUND POLARIMETRY; TRANSITIONS AB The Cosmology Large Angular Scale Surveyor (CLASS) is a ground-based instrument that will measure the polarization of the cosmic microwave background to search for evidence for gravitational waves from a posited epoch of inflation early in the Universe's history. This measurement will require integration of superconducting transition-edge sensors with microwave waveguide inputs with excellent control of systematic errors, such as unwanted coupling to stray signals at frequencies outside of a precisely defined microwave band. To address these needs, we present work on the fabrication of micromachined silicon, producing conductive quarter-wave backshort assemblies for the CLASS 40 GHz focal plane. Each 40 GHz backshort assembly consists of three degeneratively doped silicon wafers. Two spacer wafers are micromachined with through-wafer vias to provide a 2.04-mm-long square waveguide delay section. The third wafer terminates the waveguide delay in a short. The three wafers are bonded at the wafer level by Au-Au thermal compression bonding then aligned and flip chip bonded to the CLASS detector at the chip level. The micromachining techniques used have been optimized to create high aspect ratio waveguides, silicon pillars, and relief trenches with the goal of providing improved out of band signal rejection. We will discuss the fabrication of integrated CLASS superconducting detector chips with the quarter-wave backshort assemblies. C1 [Crowe, Erik J.; Chuss, David T.; Denis, Kevin L.; Moseley, Samuel H.; Rostem, Karwan; Stevenson, Thomas R.; Towner, Deborah; U-yen, Kongpop; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Crowe, Erik J.; Towner, Deborah] MEI Technol, Greenbelt, MD 20771 USA. [Bennett, Charles L.; Eimer, Joseph; Marriage, Tobias] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Crowe, EJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM erik.j.crowe@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA FX This work was supported in part by a NASA "Research Opportunities in Space and Earth Sciences" Grant. NR 15 TC 3 Z9 3 U1 0 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2500505 DI 10.1109/TASC.2012.2237211 PN 1 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100072 ER PT J AU Porst, JP Bandler, SR Adams, JS Balvin, M Beyer, J Busch, SE Drung, D Eckart, ME Kelley, RL Kilbourne, CA Porter, FS Sadleir, JE Seidel, GM Smith, SJ Stevenson, TR AF Porst, Jan-Patrick Bandler, Simon R. Adams, Joseph S. Balvin, Manuel Beyer, Joern Busch, Sarah E. Drung, Dietmar Eckart, Megan E. Kelley, Richard L. Kilbourne, Caroline A. Porter, Frederick S. Sadleir, John E. Seidel, George M. Smith, Stephen J. Stevenson, Thomas R. TI Time Domain Multiplexed Readout of Magnetically Coupled Calorimeters SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Low-temperature detectors; magnetic calorimeter; SQUID; time domain multiplexing (TDM); X-ray spectroscopy ID HIGH-RESOLUTION; MICROCALORIMETERS; PERFORMANCE; CIRCUIT; ARRAYS AB Magnetically coupled calorimeters (MCC) have extremely high potential for X-ray applications. Although very high energy-resolution has been demonstrated, until now there has been no multiplexed read-out of MCCs. We report on the first realization of a time domain multiplexed read-out of MCCs. Although this has many similarities with time domain multiplexing of transition-edge sensors, for MCCs the energy resolution is limited by the SQUID read-out noise, and requires the well established scheme to be altered in order to minimize degradation due to noise aliasing effects. In our approach, each pixel is read out by a single first-stage SQUID that is operated in open loop. The outputs of the SQ1s are low-pass filtered with an array of low cross-talk inductors, then fed into a single-stage SQUID multiplexer. The multiplexer is addressed from room temperature and read out through a single amplifier channel. We present the noise performance and compare to expectations. We have demonstrated multiplexed X-ray spectroscopy at 5.9 keV and for improved read-out noise achieved an energy resolution Delta E-FWHM < 6 eV for emulated multiplexing. We show that in an optimized setup, it is possible to multiplex 32 detectors without significantly degrading the intrinsic detector resolution. C1 [Porst, Jan-Patrick; Seidel, George M.] Brown Univ, Providence, RI 02912 USA. [Porst, Jan-Patrick; Bandler, Simon R.; Adams, Joseph S.; Balvin, Manuel; Busch, Sarah E.; Eckart, Megan E.; Kelley, Richard L.; Kilbourne, Caroline A.; Porter, Frederick S.; Sadleir, John E.; Smith, Stephen J.; Stevenson, Thomas R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bandler, Simon R.; Adams, Joseph S.; Eckart, Megan E.; Smith, Stephen J.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Beyer, Joern; Drung, Dietmar] Phys Tech Bundesanstalt, D-10587 Berlin, Germany. RP Porst, JP (reprint author), Brown Univ, Providence, RI 02912 USA. EM jp.porst@nasa.gov RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Porter, Frederick/D-3501-2012 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Porter, Frederick/0000-0002-6374-1119 FU NASA (Office of Space Science) [NNX12AL50G]; NASA Postdoctoral Program at Goddard Space Flight Center; NASA FX This work was supported by NASA (Office of Space Science, Contract NNX12AL50G from ROSES 2011). S. E. Bush was supported in part by a NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 19 TC 5 Z9 5 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2500905 DI 10.1109/TASC.2013.2243792 PN 1 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100076 ER PT J AU Sadleir, JE Smith, SJ Bandler, SR Adams, JS Busch, SE Eckart, ME Chervenak, JA Kelley, RL Kilbourne, CA Porter, FS Porst, JP Clem, JR AF Sadleir, John E. Smith, Stephen J. Bandler, Simon R. Adams, Joseph S. Busch, Sarah E. Eckart, Megan E. Chervenak, James A. Kelley, Richard L. Kilbourne, Caroline A. Porter, Frederick S. Porst, Jan-Patrick Clem, John R. TI Magnetically Tuned Superconducting Transition-Edge Sensors SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Low temperature detectors; micro calorimeter; micro calorimetry; superconducting transition-edge sensors (TESs); X-ray spectroscopy AB In this work we present a detector model for superconducting transition-edge sensors (TESs) that includes for the first time the magnetic field dependence of the resistive transition. By writing the resistance R as a function of temperature T current I and magnetic field B we present a general result requiring few assumptions that offers a new strategy to improve TES performance. Application of our TES models that agree with measurements of the critical current on TES sensors predicts that it is possible to design and operate a TES in a new regime by magnetically tuning the resistive transition surface R(T, I, B). We show using all realizable device parameter values that this new magnetically tuned transition surface is predicted to give a sensor with larger signal size, faster speed capability, reduced performance limiting Johnson noise, and improved energy resolution; and do so over the entire pulse trajectory in R(T, I, B) space. We emphasize that our result is robust in that the performance benefits listed do not hinge on a precise functional form of the resistive transition. This magnetic tuning technique can improve performance for TESs governed by a wide range of resistive mechanisms such as weakly coupled to strongly coupled superconductors or nonequilibrium superconductivity. C1 [Sadleir, John E.; Porst, Jan-Patrick] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, Stephen J.; Bandler, Simon R.; Adams, Joseph S.; Busch, Sarah E.; Eckart, Megan E.; Chervenak, James A.; Kelley, Richard L.; Kilbourne, Caroline A.; Porter, Frederick S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20742 USA. [Smith, Stephen J.; Bandler, Simon R.; Adams, Joseph S.; Eckart, Megan E.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Porst, Jan-Patrick] Brown Univ, Providence, RI 02906 USA. [Clem, John R.] Iowa State Univ, Ames, IA 50011 USA. RP Sadleir, JE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM john.e.sadleir@nasa.gov RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Porter, Frederick/D-3501-2012 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Porter, Frederick/0000-0002-6374-1119 FU U.S. Department of Energy, Office of Basic Energy Science, Division of Materials Sciences and Engineering; U.S. Department of Energy [DE-AC02-07CH11358] FX John R. Clem's research was supported by the U.S. Department of Energy, Office of Basic Energy Science, Division of Materials Sciences and Engineering, and was performed at the Ames Laboratory, which is operated for the U.S. Department of Energy by Iowa State University under Contract No. DE-AC02-07CH11358. NR 8 TC 5 Z9 5 U1 1 U2 18 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2101405 DI 10.1109/TASC.2013.2251391 PN 1 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100052 ER PT J AU Stevenson, TR Balvin, MA Bandler, SR Busch, SE Denis, KL Hsieh, WT Kelly, DP Merrell, W Nagler, PC Porst, JP Sadleir, JE Seidel, GM Smith, SJ AF Stevenson, T. R. Balvin, M. A. Bandler, S. R. Busch, S. E. Denis, K. L. Hsieh, W. -T. Kelly, D. P. Merrell, W. Nagler, P. C. Porst, J. -P. Sadleir, J. E. Seidel, G. M. Smith, S. J. TI Superconducting Effects in Optimization of Magnetic Penetration Thermometers for X-Ray Microcalorimeters SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Superconducting films; superconducting photodetectors; X-ray detection ID FIELD DEPENDENCE; GAP AB We have made high-resolution X-ray microcalorimeters using superconducting MoAu bilayers and Nb meander coils. The temperature sensor is a magnetic penetration thermometer. Operation is similar to metallic magnetic calorimeters, but instead of the magnetic susceptibility of a paramagnetic alloy, we use the diamagnetic response of the superconducting MoAu to sense temperature changes in an X-ray absorber. Flux-temperature responsivity can be large for small sensor heat capacity, with enough dynamic range for applications. We find that models of observed flux-temperature curves require several effects to explain flux penetration or expulsion in the microscopic devices. The superconductor is nonlocal, with large coherence length and weak pinning of flux. At the lowest temperatures, behavior is dominated by screening currents that vary as a result of the temperature dependence of the magnetic penetration depth, modified by the effect of the nonuniformity of the applied field occurring on a scale comparable to the coherence length. In the temperature regime where responsivity is greatest, spatial variations in the order parameter become important: both local variations as flux enters/leaves the film and an intermediate state is formed, and globally as changing stability of the electrical circuit creates a Meissner transition and flux is expelled/penetrates to minimize free energy. C1 [Stevenson, T. R.; Balvin, M. A.; Denis, K. L.; Hsieh, W. -T.; Sadleir, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bandler, S. R.] Univ Maryland, College Pk, MD 20742 USA. [Busch, S. E.; Merrell, W.] Oak Ridge Associated Univ, Oak Ridge, TN 37830 USA. [Kelly, D. P.] MEI Technol, Seabrook, MD 20706 USA. [Nagler, P. C.; Porst, J. -P.; Seidel, G. M.] Brown Univ, Providence, RI 02912 USA. [Smith, S. J.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. RP Stevenson, TR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM thomas.r.stevenson@nasa.gov; Manuel.A.Balvin@nasa.gov; simon.r.bandler@nasa.gov; sarah.e.busch@nasa.gov; Kevin.L.Denis@nasa.gov; wen-ting.hsieh-1@nasa.gov; daniel.p.kelly@nasa.gov; willie.merrell@gmail.com; peter.c.nagler@nasa.gov; porst@nasa.gov; john.e.sadleir@nasa.gov; George_Seidel@brown.edu; stephen.j.smith@nasa.gov RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106 FU NASA ROSES [NNX12AL50G]; GSFC IRAD; appointments to the NASA Postdoctoral Program FX This work was supported by NASA ROSES grant NNX12AL50G, the GSFC IRAD program, and appointments to the NASA Postdoctoral Program administered by Oak Ridge Associated Universities. NR 21 TC 0 Z9 0 U1 1 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2300605 DI 10.1109/TASC.2013.2239695 PN 1 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100065 ER PT J AU Rai, MM AF Rai, Man Mohan TI Flow physics in the turbulent near wake of a flat plate SO JOURNAL OF FLUID MECHANICS LA English DT Article DE turbulence simulation; vortex shedding; wakes ID DIRECT NUMERICAL-SIMULATION; CIRCULAR-CYLINDER; CHANNEL FLOW; TRANSPORT AB The symmetric near wake of a flat plate with a circular trailing edge, exhibiting pronounced shedding of wake vortices, is investigated via a direct numerical simulation. The separating plate boundary layers are turbulent and statistically identical. The present study focuses on the vortical structures, the distribution of phase-averaged velocity statistics and vorticity fluctuations in the near wake. Braid and vortex core regions are investigated via contours of instantaneous vorticity and pressure with an emphasis on the three-dimensionality of near-wake structures. Rib vortices are observed in the braids. The vortex cores are populated with both ribs that wrap themselves around the cores and spanwise-elongated regions of spanwise vorticity near the centres of the cores. Production terms in the transport equations for phase-averaged fluctuating vorticity show that stretching of rib vortices via the phase-averaged strain rate produces significantly less turbulent vorticity than turbulent stretching in the braids and cores. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Rai, MM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM man.m.rai@nasa.gov NR 21 TC 2 Z9 2 U1 1 U2 9 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 J9 J FLUID MECH JI J. Fluid Mech. PD JUN PY 2013 VL 724 BP 704 EP 733 DI 10.1017/jfm.2013.185 PG 30 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 144DW UT WOS:000318920800030 ER PT J AU Sun, WB Liu, ZY Lin, B Huang, JP Videen, G AF Sun, Wenbo Liu, Zhaoyan Lin, Bing Huang, Jianping Videen, Gorden TI The 2nd International Symposium on Atmospheric Light Scattering and Remote Sensing (ISALSaRS'11) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material C1 [Lin, Bing] NASA, Langley Res Ctr, Washington, DC 20546 USA. [Huang, Jianping] Lanzhou Univ, Lanzhou 730000, Peoples R China. [Videen, Gorden] USA, Res Lab, Washington, DC 20546 USA. EM wenbo.sun-1@nasa.gov NR 0 TC 1 Z9 1 U1 1 U2 5 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 JUN PY 2013 VL 122 SI SI BP 1 EP 2 DI 10.1016/j.jqsrt.2012.12.005 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 142VN UT WOS:000318825800001 ER PT J AU Kawamoto, K Suzuki, K AF Kawamoto, Kazuaki Suzuki, Kentaroh TI Comparison of water cloud microphysics over mid-latitude land and ocean using CloudSat and MODIS observations SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Cloud microphysics; Drizzle; Precipitation; CloudSat; MODIS ID NUMBER CONCENTRATION; CLIMATE; GROWTH AB The microphysical properties and processes of water (liquid-phase) clouds in the mid-latitudes were studied using space-borne radar and radiometer data, with a focus on comparisons between continental (over China) and oceanic (over the northwest Pacific) clouds. The probability distribution functions (PDFs) of cloud parameters were examined and found to be both reasonable and consistent with previous observations. The PDFs of oceanic cloud parameters as a function of radar reflectivity were generally better defined than those of land cloud parameters. Precipitation characteristics were categorized into non-precipitating, drizzle, and precipitating, as well as the total-precipitating category, according to the maximum radar reflectivity within the cloud layer. The fractional occurrence of the precipitation categories was analyzed as a function of the liquid water path. The statistics showed general trends that were very similar for both land and oceanic clouds, such as a monotonically decreasing trend for the non-precipitating category, a convex shape for the drizzle category, and a monotonically increasing trend for the precipitating and total-precipitating categories with increasing liquid water path. The fractional occurrence of the precipitation categories was further investigated as a function of multiple cloud parameters to better understand land-ocean contrasts in cloud development stages. The vertical structure of clouds also revealed that oceanic clouds produced heavier precipitation in optically thicker regions, compared to land clouds with fewer cloud droplets. However, the differences between land and oceanic clouds were small when comparisons included only those clouds with a high density of droplets. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Kawamoto, Kazuaki] Nagasaki Univ, Grad Sch Fisheries Sci & Environm Studies, Nagasaki 8528521, Japan. [Suzuki, Kentaroh] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kawamoto, K (reprint author), Nagasaki Univ, Grad Sch Fisheries Sci & Environm Studies, 1-14 Bunkyo Machi, Nagasaki 8528521, Japan. EM kazukawa@nagasaki-u.ac.jp RI Suzuki, Kentaroh/C-3624-2011 FU Mitsui Co., Ltd.; National Aeronautics and Space Administration FX K. Kawamoto was supported by the Mitsui & Co., Ltd., Environment Fund, Grant-in aid for Scientific Research (B) and Grant-in aid for Scientific Research on Innovative Areas. The CloudSat data products of 2B-GEOPROF and MODIS-AUX and ECMWF-AUX were provided by the CloudSat Data Processing Center at CIRA/Colorado State University. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 30 TC 5 Z9 6 U1 2 U2 14 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 JUN PY 2013 VL 122 SI SI BP 13 EP 24 DI 10.1016/j.jqsrt.2012.12.013 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 142VN UT WOS:000318825800003 ER PT J AU Wu, D Tang, JY Liu, ZY Hu, YX AF Wu, Dong Tang, Jiayuan Liu, Zhaoyan Hu, Yongxiang TI Simulation of coherent Doppler wind lidar measurement from space based on CALIPSO lidar global aerosol observations SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE CALIPSO lidar; Coherent Doppler wind lidar; Performance simulation; Aerosol backscatter ID PERFORMANCE; ESTIMATORS; SYSTEM; RADAR; MIE AB The performance of a space-based 2.1-mu m coherent Doppler wind lidar (CDWL) measurement at a single laser shot in clear-air conditions is computer simulated, based on the coherent Doppler lidar theory developed in the recent decades, and using the global aerosol distribution derived from one year (March 2007-February 2008) of the CALIPSO lidar measurements. The accuracy of radial wind velocity good estimates and the fraction of good estimates, depending on backscattered signals from aerosols, generally decrease with altitude. A critical altitude is defined as the altitude below which the good estimate fraction of velocity estimates is larger than 90.0%. With a laser pulse energy of 250 mJ at an off-nadir pointing angle of 45 degrees, a telescope of 1 m in diameter and a vertical range resolution of similar to 800 m, this critical altitude can reach an altitude of 4.0-5.0 km between 20 degrees S and 40 degrees N where dust and biomass burning aerosols are ubiquitous. The critical altitude gradually decreases as approaching the two poles and drops to 0.5-1.5 km in the polar regions. When the laser pulse energy is reduced to 100 mJ, the critical altitude is generally decreased by similar to 0.5 km and can still reach an altitude of 3.5-4.5 km in the dust and smoke aerosol enriched tropical and subtropical regions. A laser pulse energy of only a few millijoules can still achieve velocity measurements with an RMS error smaller than 1 m s(-1) and a good estimate fraction better than 90% in the lowest kilometers of the troposphere. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Wu, Dong; Tang, Jiayuan] Ocean Univ China, Coll Informat Sci & Engn, Qingdao 266100, Peoples R China. [Liu, Zhaoyan] Sci Syst & Applicat Inc, Hampton, VA 23681 USA. [Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Wu, D (reprint author), Ocean Univ China, Coll Informat Sci & Engn, Qingdao 266100, Peoples R China. EM dongwu@ouc.edu.cn RI Liu, Zhaoyan/B-1783-2010; Hu, Yongxiang/K-4426-2012 OI Liu, Zhaoyan/0000-0003-4996-5738; FU National Natural Science Foundations of China [40876017, 41076116, 41228008] FX This work is supported by the National Natural Science Foundations of China (Grant nos.40876017, 41076116, and 41228008). The authors acknowledge the Atmospheric Science Data Center (ASDC) at the NASA Langley Research Center for providing the CALIPSO data used in this paper. They sincerely thank Dr. Michael Kavaya at the NASA Langley Research Center for the useful discussions about the latest progress of the heterodyne detection theory. They are also grateful to two anonymous reviewers for their constructive comments. NR 29 TC 1 Z9 3 U1 1 U2 16 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 JUN PY 2013 VL 122 SI SI BP 79 EP 86 DI 10.1016/j.jqsrt.2012.11.017 PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 142VN UT WOS:000318825800009 ER PT J AU Zhang, TP Stackhouse, PW Gupta, SK Cox, SJ Mikovitz, JC Hinkelman, LM AF Zhang, Taiping Stackhouse, Paul W., Jr. Gupta, Shashi K. Cox, Stephen J. Mikovitz, J. Colleen Hinkelman, Laura M. TI The validation of the GEWEX SRB surface shortwave flux data products using BSRN measurements: A systematic quality control, production and application approach SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Solar radiation; Satellite; BSRN; GEWEX SRB; Validation ID RADIATION BUDGET; SOLAR-RADIATION; SATELLITE DATA; ISCCP; ATMOSPHERE; SCALE AB The NASA/GEWEX Surface Radiation Budget (SRB) project has produced a 24.5-year continuous record of global shortwave and longwave radiation fluxes at TOA and the Earth's surface from satellite measurements. The time span of the data is from July 1983 to December 2007, and the spatial resolution is 1 degrees latitude x 1 degrees longitude. The inputs of the latest version (Release 3.0) include the GEOS Version 4.0.3 meteorological information and cloud properties derived from ISCCP DX data. The SRB products are available on 3-hourly, 3-hourly-monthly, daily and monthly time scales. To assess the quality of the product, we extensively validated the SRB data against 5969 site-months of ground-based measurements from 52 Baseline Surface Radiation Network (BSRN) stations. This paper describes first the characteristics of the BSRN data and the GEWEX SRB data, the methodology for quality control and processing of the shortwave BSRN data, and then the systematic SRB-BSRN comparisons. It is found that, except for occasional extreme outliers as seen in scatter plots, the satellite-based surface radiation data generally agree very well with BSRN measurements. Specifically, the bias/RMS for the daily and monthly mean shortwave fluxes are, respectively, -3.6/35.5 and -5.2/23.3 W degrees m(-2) under all-sky conditions. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Zhang, Taiping; Gupta, Shashi K.; Cox, Stephen J.; Mikovitz, J. Colleen] SSA NASA Langley Res Ctr, Hampton, VA 23666 USA. [Stackhouse, Paul W., Jr.] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Hinkelman, Laura M.] Univ Washington, JISAO, Seattle, WA 98195 USA. RP Zhang, TP (reprint author), SSA NASA Langley Res Ctr, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. EM Taiping.Zhang@NASA.gov; Paul.W.Stackhouse@NASA.gov RI Hinkelman, Laura/L-8964-2016 OI Hinkelman, Laura/0000-0001-6477-9648 FU NASA Earth Science Mission, Radiation Science Program; Earth Science Mission FX The authors wish to acknowledge the fruitful discussions with Dr. Ellsworth G. Dutton and Dr. Chuck N. Long that contributed to this work. We especially want to acknowledge the leadership of Dr. Dutton over the BSRN program, in the light of his untimely death, without which this work would have been impossible. This work was funded under the NASA Earth Science Mission, Radiation Science Program, Dr. Hal Maring, program manager. Additional funding for data production and archival came from the Earth Science Mission, Dr. Jack Kaye. NR 35 TC 18 Z9 18 U1 0 U2 13 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 JUN PY 2013 VL 122 SI SI BP 127 EP 140 DI 10.1016/j.jqsrt.2012.10.004 PG 14 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 142VN UT WOS:000318825800014 ER PT J AU Yang, YK Marshak, A Mao, JP Lyapustin, A Herman, J AF Yang, Yuekui Marshak, Alexander Mao, Jianping Lyapustin, Alexei Herman, Jay TI A method of retrieving cloud top height and cloud geometrical thickness with oxygen A and B bands for the Deep Space Climate Observatory (DSCOVR) mission: Radiative transfer simulations SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE DSCOVR; L1 Lagrangian point; EPIC; Radiative transfer; Cloud top; Cloud thickness; O-2 A-band; O-2 B-band ID A-BAND; SOLAR-RADIATION; PRESSURE; ABSORPTION; SCATTERING; ALGORITHM; POLDER; MERIS AB The Earth Polychromatic Imaging Camera (EPIC) onboard the Deep Space Climate Observatory (DSCOVR) was designed to measure the atmosphere and surface properties over the whole sunlit half of the Earth from the L1 Lagrangian point. It has 10 spectral channels ranging from the UV to the near-IR, including two pairs of oxygen (O-2) A-band (779.5 and 764 nm) and B-band (680 and 687.75 nm) reference and absorption channels selected for the cloud height measurements. This paper presents the radiative transfer analysis pertinent to retrieving cloud top height and cloud geometrical thickness with EPIC A- and B-band observations. Due to photon cloud penetration, retrievals from either O-2 A- or B-band channels alone gives the corresponding cloud centroid height, which is lower than the cloud top. However, we show both the sum and the difference between the retrieved cloud centroid heights in the A and B bands are functions of cloud top height and cloud geometrical thickness. Based on this fact, the paper develops a new method to retrieve cloud top height and cloud geometrical thickness simultaneously for fully cloudy scenes over ocean surface. First, cloud centroid heights are calculated for both A and B bands using the ratios between the reflectances of the absorbing and reference channels; then the cloud top height and the cloud geometrical thickness are retrieved from the two dimensional look up tables that relate the sum and the difference between the retrieved centroid heights for A and B bands to the cloud top height and the cloud geometrical thickness. This method is applicable for clouds thicker than an optical depth of 5. Published by Elsevier Ltd. C1 [Yang, Yuekui] Univ Space Res Assoc, Columbia, MD USA. [Yang, Yuekui; Marshak, Alexander; Mao, Jianping; Lyapustin, Alexei; Herman, Jay] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mao, Jianping] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Herman, Jay] UMBC, Joint Ctr Earth Syst Technol, Baltimore, MD USA. RP Yang, YK (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA. EM Yuekui.Yang@nasa.gov RI Marshak, Alexander/D-5671-2012; Lyapustin, Alexei/H-9924-2014; Yang, Yuekui/B-4326-2015; OI Lyapustin, Alexei/0000-0003-1105-5739; Herman, Jay/0000-0002-9146-1632 FU NASA DSCOVR FX We thank two anonymous reviewers for reviewing this manuscript and for their insightful comments. This study is supported by the NASA DSCOVR refurbishement project. NR 30 TC 7 Z9 7 U1 1 U2 16 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 JUN PY 2013 VL 122 SI SI BP 141 EP 149 DI 10.1016/j.jqsrt.2012.09.017 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 142VN UT WOS:000318825800015 ER PT J AU Lin, B Stackhouse, P Sun, WB Hu, YX Liu, ZY Fan, TF AF Lin, Bing Stackhouse, Paul, Jr. Sun, Wenbo Hu, Yongxiang Liu, Zhaoyan Fan, Tai-Fang (Alice) TI Is Oklahoma getting drier? SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Satellite remote sensing; Soil moisture; Surface radiation; Precipitation; Surface latent and sensible heat; Surface temperature; In-situ measurement ID SOIL-MOISTURE VARIABILITY; GLOBAL PRECIPITATION; DYNAMICS; NETWORK; BUDGET; TOP AB Land surface hydrology is important to regional climate, ecosystem, agriculture, and even human activities. Changes in soil moisture can produce considerable impacts on socioeconomics. Analysis of assimilation model results, especially those from the Community Land Model, shows that soil moisture over Oklahoma region is continuously reduced from 1980 to 2009. The potential drying trend in the Oklahoma region is evaluated by observations taken during last three decades in this study. Satellite data from Global Precipitation Climatology Project exhibit a clear precipitation decrease in the Oklahoma region during the last decade or so compared with those of two or three decades ago. Accompanying with the precipitation variation, land surface net radiation and temperature over the region are found increases by satellite and/or in-situ measurements. These changes in regional climate conditions also likely result in reduction of regional evaporation and enhancement of sensible heat transport from land surface into the atmosphere as indicated in assimilated data. These observed and modeled evidences of the changes in regional water and energy cycles lead us to conclude that the soil moisture over the Oklahoma region was reduced during the last decade. This soil moisture drop could increase a risk in water shortage for agriculture in the Oklahoma state if the dry period continues. Further investigations on the drying in the Oklahoma State or even entire Southern Great Plains are needed to mitigate potential droughts, reductions in vegetation products, and other socioeconomic impacts. Published by Elsevier Ltd. C1 [Lin, Bing; Stackhouse, Paul, Jr.; Hu, Yongxiang] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Sun, Wenbo; Liu, Zhaoyan; Fan, Tai-Fang (Alice)] SSAI, Hampton, VA 23666 USA. RP Lin, B (reprint author), NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. EM bing.lin@nasa.gov RI Liu, Zhaoyan/B-1783-2010; Hu, Yongxiang/K-4426-2012 OI Liu, Zhaoyan/0000-0003-4996-5738; FU NASA Energy and Water cycle Studies (NEWS) program; CERES mission FX The authors would like to express their appreciation to M. Rodell and G. Huffman for their expertise in assimilated and precipitation data, respectively. L. Smith, D. Garber, G. Gibson, and N. Loeb provide invaluable comments. This research was supported by the NASA Energy and Water cycle Studies (NEWS) program and CERES mission. CERES and SRB products and land surface data were obtained from the NASA Langley Atmospheric Sciences Data Center in Hampton, Virginia and Goddard Distributed Active Archive Center in Greenbelt, Maryland, respectively. NR 26 TC 0 Z9 0 U1 1 U2 18 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 JUN PY 2013 VL 122 SI SI BP 208 EP 213 DI 10.1016/j.jqsrt.2012.07.024 PG 6 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 142VN UT WOS:000318825800021 ER PT J AU Sun, WB Liu, ZY Videen, G Fu, Q Muinonen, K Winker, DM Lukashin, C Jin, ZH Lin, B Huang, JP AF Sun, Wenbo Liu, Zhaoyan Videen, Gorden Fu, Qiang Muinonen, Karri Winker, David M. Lukashin, Constantine Jin, Zhonghai Lin, Bing Huang, Jianping TI For the depolarization of linearly polarized light by smoke particles SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Linearly polarized light; Depolarization ratio; Particle characterization; Smoke aerosol ID ABSORBING BOUNDARY-CONDITION; TIME-DOMAIN SOLUTION; SCATTERING; SOOT; ABSORPTION AB The CALIPSO satellite mission consistently measures volume (including molecule and particulate) light depolarization ratio of similar to 2% for smoke, compared to similar to 1% for marine aerosols and similar to 15% for dust. The observed similar to 2% smoke depolarization ratio comes primarily from the nonspherical habits of particles in the smoke at certain particle sizes. In this study, the depolarization of linearly polarized light by small sphere aggregates and irregular Gaussian-shaped particles is studied, to reveal the physics between the depolarization of linearly polarized light and smoke aerosol shape and size. It is found that the depolarization ratio curves of Gaussian-deformed spheres are very similar to sphere aggregates in terms of scattering-angle dependence and particle size parameters when particle size parameter is smaller than 1.0 pi. This demonstrates that small randomly oriented nonspherical particles have some common depolarization properties as functions of scattering angle and size parameter. This may be very useful information for characterization and active remote sensing of smoke particles using polarized light. We also show that the depolarization ratio from the CALIPSO measurements could be used to derive smoke aerosol particle size. From the calculation results for light depolarization ratio by Gaussian-shaped smoke particles and the CALIPSO-measured light depolarization ratio of similar to 2% for smoke, the mean particle size of South-African smoke is estimated to be about half of the 532 nm wavelength of the CALIPSO lidar. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Sun, Wenbo; Liu, Zhaoyan; Jin, Zhonghai] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Videen, Gorden] USA, Res Lab, Adelphi, MD 20783 USA. [Fu, Qiang] Univ Washington, Seattle, WA 98195 USA. [Muinonen, Karri] Univ Helsinki, FIN-00014 Helsinki, Finland. [Sun, Wenbo; Winker, David M.; Lukashin, Constantine; Lin, Bing] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Huang, Jianping] Lanzhou Univ, Lanzhou 730000, Peoples R China. RP Sun, WB (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM wenbo.sun-1@nasa.gov RI Liu, Zhaoyan/B-1783-2010; Richards, Amber/K-8203-2015 OI Liu, Zhaoyan/0000-0003-4996-5738; FU NASA [09-GLORY09-0027]; NASA CLARREO mission FX This work was supported by NASA Glory fund 09-GLORY09-0027 and partially by NASA CLARREO mission. The authors thank Michael I. Mishchenko, Hal B. Maring, Bruce A. Wielicki, and Dave F. Young for their support on this work. NR 23 TC 11 Z9 12 U1 2 U2 13 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 JUN PY 2013 VL 122 SI SI BP 233 EP 237 DI 10.1016/j.jqsrt.2012.03.031 PG 5 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 142VN UT WOS:000318825800023 ER PT J AU Moorthy, KK Beegum, SN Srivastava, N Satheesh, SK Chin, M Blond, N Babu, SS Singh, S AF Moorthy, K. Krishna Beegum, S. Naseema Srivastava, N. Satheesh, S. K. Chin, Mian Blond, Nadege Babu, S. Suresh Singh, S. TI Performance evaluation of chemistry transport models over India SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosols; Black carbon; Chemistry transport models ID AEROSOL BLACK CARBON; ATMOSPHERIC BOUNDARY-LAYER; TROPICAL COASTAL STATION; LIGHT-ABSORPTION; GOCART MODEL; AIRBORNE MEASUREMENTS; AIRCRAFT MEASUREMENTS; OPTICAL-PROPERTIES; URBAN LOCATION; DUST AEROSOLS AB Using continuous and near-real time measurements of the mass concentrations of black carbon (BC) aerosols near the surface, for a period of 1 year (from January to December 2006) from a network of eight observatories spread over different environments of India, a space-time synthesis is generated. The strong seasonal variations observed, with a winter high and summer low, are attributed to the combined effects of changes in synoptic air mass types, modulated strongly by the atmospheric boundary layer dynamics. Spatial distribution shows much higher BC concentration over the Indo-Gangetic Plain (IGP) than the peninsular Indian stations. These were examined against the simulations using two chemical transport models, GOCART (Goddard Global Ozone Chemistry Aerosol Radiation and Transport) and CHIMERE for the first time over Indian region. Both the model simulations significantly deviated from the measurements at all the stations; more so during the winter and pre-monsoon seasons and over mega cities. However, the CHIMERE model simulations show better agreement compared with the measurements. Notwithstanding this, both the models captured the temporal variations; at seasonal and subseasonal timescales and the natural variabilities (intra-seasonal oscillations) fairly well, especially at the off-equatorial stations. It is hypothesized that an improvement in the atmospheric boundary layer (ABL) parameterization scheme for tropical environment might lead to better results with GOCART. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Moorthy, K. Krishna; Beegum, S. Naseema; Babu, S. Suresh] Vikram Sarabhai Space Ctr, Space Phys Lab, Thiruvananthapuram 695022, Kerala, India. [Beegum, S. Naseema; Singh, S.] CSIR, Natl Phys Lab, Radio & Atmospher Sci Div, New Delhi 110012, India. [Srivastava, N.; Satheesh, S. K.] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India. [Satheesh, S. K.] Indian Inst Sci, Divecha Ctr Climate Change, Bangalore 560012, Karnataka, India. [Chin, Mian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blond, Nadege] Fac Geog & Amenagement, ERL 7230, Lab Image Ville Environm, F-67000 Strasbourg, France. RP Satheesh, SK (reprint author), Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India. EM satheesh@caos.iisc.ernet.in RI Chin, Mian/J-8354-2012; Singh, Sachchidanand/D-1537-2009; OI Singh, Sachchidanand/0000-0003-0257-4705; Moorthy, K. Krishna/0000-0002-7234-3868 FU Department of Science and Technology (DST), New Delhi FX The work is carried out as a part of the ARFI project of ISRO-GBP. The authors are grateful to the investigators P.C.S Devara (Pune), Biswadip Khare (Hyderbad), and UC Dumka (Nainital) for supporting the measurements. One of the authors (SKS) would like to thank Department of Science and Technology (DST), New Delhi for Swarna Jayanti fellowship. NR 80 TC 23 Z9 23 U1 2 U2 24 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD JUN PY 2013 VL 71 BP 210 EP 225 DI 10.1016/j.atmosenv.2013.01.056 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 136SY UT WOS:000318384900025 ER PT J AU Siegal, PH AF Siegal, Peter H. TI Report on Photonics West Show SO IEEE MICROWAVE MAGAZINE LA English DT Article C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Siegal, PH (reprint author), CALTECH, Jet Prop Lab, MS 168-3264800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1527-3342 J9 IEEE MICROW MAG JI IEEE Microw. Mag. PD JUN PY 2013 VL 14 IS 4 BP 167 EP 167 DI 10.1109/MMM.2013.2248674 PG 1 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 141ZE UT WOS:000318764400017 ER PT J AU Hoonakker, PLT Carayon, P McGuire, K Khunlertkit, A Wiegmann, DA Alyousef, B Xie, AP Wood, KE AF Hoonakker, Peter L. T. Carayon, Pascale McGuire, Kerry Khunlertkit, Adjhaporn Wiegmann, Douglas A. Alyousef, Bashar Xie, Anping Wood, Kenneth E. TI Motivation and job satisfaction of Tele-ICU nurses SO JOURNAL OF CRITICAL CARE LA English DT Article DE Intensive Care Unit; Tele-nursing; Organization and administration ID CARE-UNIT TELEMEDICINE; PARADIGM AB Introduction: Although the first tele-ICU has been in existence for more than 12 years, little is known about the work of tele-ICU nurses. This study examines sources of motivation and satisfaction of tele-ICU nurses. Methods: A total of 50 nurses in 5 tele-ICUs were interviewed about reasons for working as a tele-ICU nurse and sources of satisfaction and dissatisfaction in their job. Results: Nurses have different motivations to work in the tele-ICU, including the challenges and opportunities for new learning that occur while interacting with clinicians in the tele-ICU and the various ICUs being monitored. Tele-ICU nurses also appreciate the opportunities for teamwork with tele-ICU physicians and nurses. The relationship and interactions with the ICUs is sometimes mentioned as a dissatisfier. Some nurses miss being physically at the bedside, as well as interacting with patients and families. Conclusion: Most tele-ICU nurses are satisfied with their job. They like the challenge in their work and the opportunity to learn. For some nurses, the transition from a bedside caregiver to an information manager can be difficult. Other nurses have found a balance by working part-time in the tele-ICU and part-time in the ICU. (c) 2013 Elsevier Inc. All rights reserved. C1 [Hoonakker, Peter L. T.; Carayon, Pascale; Wiegmann, Douglas A.; Alyousef, Bashar; Xie, Anping] Univ Wisconsin, CQPI, Madison, WI 53706 USA. [Carayon, Pascale; Wiegmann, Douglas A.; Alyousef, Bashar; Xie, Anping] Univ Wisconsin, Dept Ind & Syst Engn, Madison, WI 53706 USA. [McGuire, Kerry] NASA, Johnson Space Ctr, Houston, TX 77052 USA. [Khunlertkit, Adjhaporn] Johns Hopkins Univ, Sch Med, Dept Anesthesiol & Crit Care Med, Qual & Safety Res Grp, Baltimore, MD USA. [Wood, Kenneth E.] Geisinger Hlth Syst, Danville, PA 17822 USA. RP Hoonakker, PLT (reprint author), Univ Wisconsin, CQPI, Madison, WI 53706 USA. EM phoonakker@cqpi.engr.wisc.edu RI Carayon, Pascale/M-5375-2013; Xie, Anping/J-4762-2015 OI Carayon, Pascale/0000-0003-4632-6930; FU National Science Foundation (NSF Grant) [OCI-0838513] FX This study was made possible with support from the National Science Foundation (NSF Grant #: OCI-0838513, Carayon: PI; Brown, Hoonakker, Wiegmann and Wood, co-PIs) and the cooperation from the 5 tele-ICUs, and their managers and the nurses who work there. NR 21 TC 1 Z9 1 U1 5 U2 38 PU W B SAUNDERS CO-ELSEVIER INC PI PHILADELPHIA PA 1600 JOHN F KENNEDY BOULEVARD, STE 1800, PHILADELPHIA, PA 19103-2899 USA SN 0883-9441 J9 J CRIT CARE JI J. Crit. Care PD JUN PY 2013 VL 28 IS 3 AR 315.e13 DI 10.1016/j.jcrc.2012.10.001 PG 9 WC Critical Care Medicine SC General & Internal Medicine GA 138ZW UT WOS:000318552000020 PM 23159143 ER PT J AU Romanou, A Gregg, WW Romanski, J Kelley, M Bleck, R Healy, R Nazarenko, L Russell, G Schmidt, GA Sun, S Tausnev, N AF Romanou, A. Gregg, W. W. Romanski, J. Kelley, M. Bleck, R. Healy, R. Nazarenko, L. Russell, G. Schmidt, G. A. Sun, S. Tausnev, N. TI Natural air-sea flux of CO2 in simulations of the NASA-GISS climate model: Sensitivity to the physical ocean model formulation SO OCEAN MODELLING LA English DT Article DE Carbon cycle; Climate modeling; Ocean modeling ID ANTHROPOGENIC CO2; CARBON-DIOXIDE; ADVECTION; EXCHANGE; DRIVEN; IRON AB Results from twin control simulations of the preindustrial CO2 gas exchange (natural flux of CO2) between the ocean and the atmosphere are presented here using the NASA-GISS climate model, in which the same atmospheric component (modelE2) is coupled to two different ocean models, the Russell ocean model and HYCOM. Both incarnations of the GISS climate model are also coupled to the same ocean biogeochemistry module (NOBM) which estimates prognostic distributions for biotic and abiotic fields that influence the air-sea flux of CO2. Model intercomparison is carried out at equilibrium conditions and model differences are contrasted with biases from present day climatologies. Although the models agree on the spatial patterns of the air-sea flux of CO2, they disagree on the strength of the North Atlantic and Southern Ocean sinks mainly because of kinematic (winds) and chemistry (pCO(2)) differences rather than thermodynamic (SST) ones. Biology/chemistry dissimilarities in the models stem from the different parameterizations of advective and diffusive processes, such as overturning, mixing and horizontal tracer advection and to a lesser degree from parameterizations of biogeochemical processes such as gravitational settling and sinking. The global meridional overturning circulation illustrates much of the different behavior of the biological pump in the two models, together with differences in mixed layer depth which are responsible for different SST, DIC and nutrient distributions in the two models and consequently different atmospheric feedbacks (in the wind, net heat and freshwater fluxes into the ocean). (c) 2013 Elsevier Ltd. All rights reserved. C1 [Romanou, A.; Bleck, R.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Romanou, A.; Kelley, M.; Bleck, R.; Russell, G.; Schmidt, G. A.] NASA, GISS, New York, NY USA. [Gregg, W. W.] NASA, GSFC, Greenbelt, MD USA. [Romanski, J.; Healy, R.; Nazarenko, L.; Schmidt, G. A.; Tausnev, N.] Columbia Univ, Ctr Clim Syst Res, New York, NY 10027 USA. [Sun, S.] NOAA, ESRL, Boulder, CO USA. RP Romanou, A (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA. EM ar2235@columbia.edu RI Schmidt, Gavin/D-4427-2012; Healy, Richard/J-9214-2015; Sun, Shan/H-2318-2015 OI Schmidt, Gavin/0000-0002-2258-0486; Healy, Richard/0000-0002-5098-8921; FU NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center; NASA-ROSES Modeling, Analysis and Prediction [NNH08ZDA001N-MAP] FX Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. Funding was provided by NASA-ROSES Modeling, Analysis and Prediction 2008 NNH08ZDA001N-MAP. We would like to thank Reto Ruedy for providing help with model setup and runs. The lead author would also like to thank John Marshall, John Dunne, Stephanie Dutkiewicz and Irina Marinov for very helpful and insightful discussions. NR 50 TC 8 Z9 8 U1 1 U2 23 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1463-5003 EI 1463-5011 J9 OCEAN MODEL JI Ocean Model. PD JUN PY 2013 VL 66 BP 26 EP 44 DI 10.1016/j.ocemod.2013.01.008 PG 19 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA 139TQ UT WOS:000318607900003 ER PT J AU Yu, HB Zhang, ZB AF Yu, Hongbin Zhang, Zhibo TI New Directions: Emerging satellite observations of above-cloud aerosols and direct radiative forcing SO ATMOSPHERIC ENVIRONMENT LA English DT Editorial Material DE Aerosol above clouds; Radiative forcing; Satellite remote sensing ID ABSORBING AEROSOLS; OPTICAL DEPTH; LAYERS; RETRIEVAL AB Spaceborne lidar and passive sensors with multi-wavelength, multi-angle and polarization capabilities onboard the A-Train provide unprecedented opportunities of observing above-cloud aerosols and direct radiative forcing. Significant progress has been made in recent years in exploring these new aerosol remote sensing capabilities and generating unique datasets. The emerging observations will advance the understanding of aerosol climate forcing. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Yu, Hongbin] NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. [Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA. [Zhang, Zhibo] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Yu, HB (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. EM Hongbin.Yu@gmail.com; Zhibo.Zhang@umbc.edu RI Yu, Hongbin/C-6485-2008; Zhang, Zhibo/D-1710-2010 OI Yu, Hongbin/0000-0003-4706-1575; Zhang, Zhibo/0000-0001-9491-1654 NR 25 TC 16 Z9 16 U1 3 U2 29 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 JUN PY 2013 VL 72 BP 36 EP 40 DI 10.1016/j.atmosenv.2013.02.017 PG 5 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 135BW UT WOS:000318262000005 ER PT J AU Poulain, X Kohlman, LW Binienda, W Roberts, GD Goldberg, RK Benzerga, AA AF Poulain, X. Kohlman, L. W. Binienda, W. Roberts, G. D. Goldberg, R. K. Benzerga, A. A. TI Determination of the intrinsic behavior of polymers using digital image correlation combined with video-monitored testing SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES LA English DT Article DE Plastic instability; Large strain behavior; True stress-strain measurement; Tension-compression asymmetry ID STRESS-STRAIN CURVES; GLASSY-POLYMERS; EPOXY-RESIN; PLASTIC-DEFORMATION; SOLID POLYMERS; YIELD BEHAVIOR; TENSILE; LOCALIZATION; COMPRESSION; POLYCARBONATE AB Three methods for the determination of the large-strain behavior of ductile polymers are compared in both tension and compression. Each method relies on some (non-contact) measurement of the strain and some approximations in the calculation of stress. The strain measurement techniques include digital image correlation (DIC) and two techniques of video-based extensometry: marker tracking and area variation monitoring. Since the specimens are inevitably subject to structural plastic instabilities (necking in tension, barreling in compression) the strain and stress states are no longer uniform in the gauge section after the peak load. Under such circumstances, it is demonstrated that the three experimental methods can lead to significant differences. It is inferred from the comparative analysis that the method based on vertical marker tracking is not reliable. Validated by DIC, video-based area variation is shown to be a simple alternative way to obtain an excellent estimate of the intrinsic true stress-strain behavior of the polymer. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Poulain, X.; Benzerga, A. A.] Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA. [Kohlman, L. W.; Binienda, W.] Univ Akron, Akron, OH 44325 USA. [Roberts, G. D.; Goldberg, R. K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Benzerga, A. A.] Texas A&M Univ, Mat Sci & Engn Program, College Stn, TX 77843 USA. RP Benzerga, AA (reprint author), Texas A&M Univ, Mat Sci & Engn Program, College Stn, TX 77843 USA. EM benzerga@tamu.edu RI Benzerga, Amine/K-2045-2014 OI Benzerga, Amine/0000-0002-6644-470X FU NASA Glenn Research Center [NNX07AV39A, NNX07AV60A] FX The authors acknowledge support from NASA Glenn Research Center under cooperative agreement NNX07AV39A between Texas Engineering Experiment Station and GRC, and cooperative agreement NNX07AV60A between the University of Akron and GRC. The authors would also like to thank Tim Woodburry from TAMU for his assistance with video-monitored post-processing of test results. NR 39 TC 10 Z9 10 U1 1 U2 27 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7683 J9 INT J SOLIDS STRUCT JI Int. J. Solids Struct. PD JUN 1 PY 2013 VL 50 IS 11-12 BP 1869 EP 1878 DI 10.1016/j.ijsolstr.2013.01.041 PG 10 WC Mechanics SC Mechanics GA 136UY UT WOS:000318390100002 ER PT J AU Severino, G Straus, T Oliviero, M Steffen, M Fleck, B AF Severino, G. Straus, T. Oliviero, M. Steffen, M. Fleck, B. TI The Intensity-Velocity Phase Spectra of Evanescent Oscillations and Acoustic Sources SO SOLAR PHYSICS LA English DT Article DE Helioseismology, direct modeling; Waves, modes; Velocity fields, photosphere ID LINE-PROFILES; SOLAR OSCILLATIONS; GRAVITY-WAVES; P-MODES; CONVECTION; ATMOSPHERE; SCATTERING; AMPLITUDES; DYNAMICS; STARS AB There are three major issues in modeling solar evanescent oscillations: the variation of the intensity [I]-velocity [V] phase difference of p-modes close to the base of photosphere; the existence of a plateau of negative I-V phase differences below and between the ridges of the low-frequency p-modes; the explanation of the I-V cross-spectra of the evanescent oscillations. We present new interpretations for the first two issues, based on modeling intensity fluctuations taking steep temperature gradients, opacity, and non-adiabatic cooling into account. We also discuss consequences of our model for the explanation of power spectra and cross-power spectra of p-modes. In particular, we present evidence that the acoustic sources that generate evanescent waves produce a coherent background that explains the plateau-interridge regime of negative I-V phase difference. C1 [Severino, G.; Straus, T.; Oliviero, M.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Steffen, M.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Fleck, B.] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA. RP Severino, G (reprint author), INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy. EM severino@oacn.inaf.it; straus@oacn.inaf.it; oliviero@oacn.inaf.it; msteffen@aip.de; bfleck@esa.nascom.nasa.gov OI Straus, Thomas/0000-0002-6280-806X; oliviero, maurizio/0000-0001-9939-115X FU Italian Space Agency (ASI); PRIN-INAF FX This work is dedicated to F.-L. Deubner, a pioneer of helioseismology and our master in this field. We thank the anonymous referee for making a number of very useful comments. One of the authors (GS) acknowledges financial support from the Italian Space Agency (ASI) and from the PRIN-INAF 2010 Asteroseismology: looking inside the stars with space- and ground-based observations. SDO/HMI data courtesy of NASA/SDO and the HMI science team. NR 28 TC 1 Z9 1 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2013 VL 284 IS 2 BP 297 EP 314 DI 10.1007/s11207-012-0172-9 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 138OK UT WOS:000318517800002 ER PT J AU Wolpert, DH Benford, G AF Wolpert, David H. Benford, Gregory TI The lesson of Newcomb's paradox SO SYNTHESE LA English DT Article DE Newcomb's paradox; Game theory; Bayes net; Causality; Determinism ID RESOLUTION AB In Newcomb's paradox you can choose to receive either the contents of a particular closed box, or the contents of both that closed box and another one. Before you choose though, an antagonist uses a prediction algorithm to accurately deduce your choice, and uses that deduction to fill the two boxes. The way they do this guarantees that you made the wrong choice. Newcomb's paradox is that game theory's expected utility and dominance principles appear to provide conflicting recommendations for what you should choose. Here we show that the conflicting recommendations assume different probabilistic structures relating your choice and the algorithm's prediction. This resolves the paradox: the reason there appears to be two conflicting recommendations is that the probabilistic structure relating the problem's random variables is open to two, conflicting interpretations. We then show that the accuracy of the prediction algorithm in Newcomb's paradox, the focus of much previous work, is irrelevant. We end by showing that Newcomb's paradox is time-reversal invariant; both the paradox and its resolution are unchanged if the algorithm makes its 'prediction' after you make your choice rather than before. C1 [Wolpert, David H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Benford, Gregory] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92692 USA. RP Wolpert, DH (reprint author), NASA, Ames Res Ctr, MS 269-1, Moffett Field, CA 94035 USA. EM david.h.wolpert@nasa.gov NR 22 TC 1 Z9 1 U1 2 U2 10 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0039-7857 J9 SYNTHESE JI Synthese PD JUN PY 2013 VL 190 IS 9 BP 1637 EP 1646 DI 10.1007/s11229-011-9899-3 PG 10 WC History & Philosophy Of Science; Philosophy SC History & Philosophy of Science; Philosophy GA 138CS UT WOS:000318486700010 ER PT J AU Sibonga, JD AF Sibonga, Jean D. TI Spaceflight-induced Bone Loss: Is there an Osteoporosis Risk? SO CURRENT OSTEOPOROSIS REPORTS LA English DT Article DE Quantitative computed tomography; Finite element modeling; Astronaut AB Currently, the measurement of areal bone mineral density (aBMD) is used at NASA to evaluate the effects of spaceflight on the skeletal health of astronauts. Notably, there are precipitous declines in aBMD with losses > 10 % detected in the hip and spine in some astronauts following a typical 6-month mission in space. How those percentage changes in aBMD relate to fracture risk in the youngeraged astronaut is unknown. Given the unique set of risk factors that could be contributing to this bone loss (eg, adaptation to weightlessness, suboptimal diet, reduced physical activity, perturbed mineral metabolism), one might not expect skeletal changes due to spaceflight to be similar to skeletal changes due to aging. Consequently, dual-energy Xray absorptiometry (DXA) measurement of aBMD may be too limiting to understand fracture probability in the astronaut during a long-duration mission and the risk for premature osteoporosis after return to Earth. Following a brief review of the current knowledge-base, this paper will discuss some innovative research projects being pursued at NASA to help understand skeletal health in astronauts. C1 NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Sibonga, JD (reprint author), NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM Jean.sibonga-1@NASA.gov NR 27 TC 20 Z9 24 U1 2 U2 8 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA EI 1544-2241 J9 CURR OSTEOPOROS REP JI Curr. Osteoporos. Rep. PD JUN PY 2013 VL 11 IS 2 BP 92 EP 98 DI 10.1007/s11914-013-0136-5 PG 7 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA V35YX UT WOS:000209182000004 PM 23564190 ER PT J AU Blackwell, WJ Lim, BH AF Blackwell, William J. Lim, Boon H. TI The IEEE GRSS Working Group on Remote Sensing Instruments and Technologies for Small Satellites SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE LA English DT Editorial Material C1 [Blackwell, William J.] MIT Lincoln Lab, Lexington, MA 02421 USA. [Lim, Boon H.] Jet Prop Lab, Pasadena, CA USA. RP Blackwell, WJ (reprint author), MIT Lincoln Lab, Lexington, MA 02421 USA. EM WJB@LL.MIT.EDU; bhlim@jpl.nasa.gov NR 10 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2168-6831 J9 IEEE GEOSC REM SEN M JI IEEE Geosci. Remote Sens. Mag. PD JUN PY 2013 VL 1 IS 2 BP 68 EP 70 DI 10.1109/MGRS.2013.2260912 PG 3 WC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology GA V45AS UT WOS:000209790100006 ER PT J AU Silver, KC Carroll, M AF Silver, Kirk C. Carroll, Mark TI A Comparative Review of North American Tundra Delineations SO ISPRS INTERNATIONAL JOURNAL OF GEO-INFORMATION LA English DT Review DE Tundra; ecoregion; North America; classification systems; GIS; review AB Recent profound changes have been observed in the Arctic environment, including record low sea ice extents and high latitude greening. Studying the Arctic and how it is changing is an important element of climate change science. The Tundra, an ecoregion of the Arctic, is directly related to climate change due to its effects on the snow ice feedback mechanism and greenhouse gas cycling. Like all ecoregions, the Tundra border is shifting, yet studies and policies require clear delineation of boundaries. There are many options for ecoregion classification systems, as well as resources for creating custom maps. To help decision makers identify the best classification system possible, we present a review of North American Tundra ecoregion delineations and further explore the methodologies, purposes, limitations, and physical properties of five common ecoregion classification systems. We quantitatively compare the corresponding maps by area using a geographic information system. C1 [Silver, Kirk C.] Univ Rhode Isl, Coll Environm & Life Sci, Coastal Inst MESM 106, Kingston, RI 02881 USA. [Carroll, Mark] NASA Goddard Space Flight Ctr, Sigma Space Corp, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Silver, KC (reprint author), Univ Rhode Isl, Coll Environm & Life Sci, Coastal Inst MESM 106, Kingston, RI 02881 USA. EM kirk.silver@gmail.com; mark.carroll@nasa.gov NR 89 TC 0 Z9 0 U1 2 U2 3 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2220-9964 J9 ISPRS INT GEO-INF JI ISPRS Int. Geo-Inf. PD JUN PY 2013 VL 2 IS 2 BP 324 EP 348 DI 10.3390/ijgi2020324 PG 25 WC Geography, Physical; Remote Sensing SC Physical Geography; Remote Sensing GA V40FY UT WOS:000209465700004 ER PT J AU Steltzner, A AF Steltzner, Adam TI Q&A ADAM STELTZNER SO MECHANICAL ENGINEERING LA English DT Editorial Material C1 [Steltzner, Adam] NASA, Jet Prop Lab, Pasadena, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0025-6501 EI 1943-5649 J9 MECH ENG JI Mech. Eng. PD JUN PY 2013 VL 135 IS 6 BP 20 EP 20 PG 1 WC Engineering, Mechanical SC Engineering GA AQ0PH UT WOS:000342484700013 ER PT J AU Srivastava, AN Chawla, NV AF Srivastava, Ashok N. Chawla, Nitesh V. TI Special Issue on CIDU '11 SO STATISTICAL ANALYSIS AND DATA MINING LA English DT Editorial Material C1 [Srivastava, Ashok N.] NASA, Ames Res Ctr, New York, NY USA. [Chawla, Nitesh V.] Univ Notre Dame, Notre Dame, IN 46556 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-1864 EI 1932-1872 J9 STAT ANAL DATA MIN JI Stat. Anal. Data Min. PD JUN PY 2013 VL 6 IS 3 SI SI BP 157 EP 157 DI 10.1002/sam.11194 PG 1 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Statistics & Probability SC Computer Science; Mathematics GA V41CW UT WOS:000209525300001 ER PT J AU Thompson, DR Majid, WA Reed, CJ Wagstaff, KL AF Thompson, David R. Majid, Walid A. Reed, Colorado J. Wagstaff, Kiri L. TI Semi-Supervised Eigenbasis Novelty Detection SO STATISTICAL ANALYSIS AND DATA MINING LA English DT Article DE novelty detection; time series analysis; radio astronomy; machine learning; anomaly detection; radio transients; fast transients; semi-supervised learning AB We present a semi-supervised online method for novelty detection and evaluate its performance for radio astronomy time series data. Our approach uses sparse, adaptive eigenbases to combine (1) prior knowledge about uninteresting signals with (2) online estimation of the current data properties to enable highly sensitive and precise detection of novel signals. We apply Semi-Supervised Eigenbasis Novelty Detection (SSEND) to the problem of detecting fast transient radio anomalies and compare it to current alternative algorithms. Tests based on observations from the Parkes Multibeam Survey show both effective detection of interesting rare events and robustness to known false alarm anomalies. (c) 2012 Wiley Periodicals, Inc. C1 [Thompson, David R.; Majid, Walid A.; Reed, Colorado J.; Wagstaff, Kiri L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM david.r.thompson@jpl.nasa.gov OI Wagstaff, Kiri/0000-0003-4401-5506 NR 22 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-1864 EI 1932-1872 J9 STAT ANAL DATA MIN JI Stat. Anal. Data Min. PD JUN PY 2013 VL 6 IS 3 SI SI BP 195 EP 204 DI 10.1002/sam.11148 PG 10 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Statistics & Probability SC Computer Science; Mathematics GA V41CW UT WOS:000209525300004 ER PT J AU Das, K Srivastava, AN AF Das, Kamalika Srivastava, Ashok N. TI Sparse Inverse Kernel Gaussian Process Regression SO STATISTICAL ANALYSIS AND DATA MINING LA English DT Article DE sparse regression; Gaussian processes; earth science data; ADMM AB Regression problems on massive data sets are ubiquitous in many application domains including the Internet, earth and space sciences, and finances. Gaussian Process regression (GPR) is a popular technique for modeling the input-output relations of a set of variables under the assumption that the weight vector has a Gaussian prior. However, it is challenging to apply GPR to large data sets since prediction based on the learned model requires inversion of an order n kernel matrix. Approximate solutions for sparse Gaussian Processes have been proposed for sparse problems. However, in almost all cases, these solution techniques are agnostic to the input domain and do not preserve the similarity structure in the data. As a result, although these solutions sometimes provide excellent accuracy, the models do not have interpretability. Such interpretable sparsity patterns are very important for many applications. We propose a new technique for sparse GPR that allows us to compute a parsimonious model while preserving the interpretability of the sparsity structure in the data. We discuss how the inverse kernel matrix used in Gaussian Process prediction gives valuable domain information and then adapt the inverse covariance estimation from Gaussian graphical models to estimate the Gaussian kernel. We solve the optimization problem using the alternating direction method of multipliers that is amenable to parallel computation. We compare the performance of this algorithm to different existing methods for sparse covariance regression in terms of both speed and accuracy. We demonstrate the performance of our method in terms of accuracy, scalability, and interpretability on two different satellite data sets from the climate domain. (c) 2013 Wiley Periodicals, Inc. C1 [Das, Kamalika] Univ Calif Santa Cruz, UARC, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Srivastava, Ashok N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Das, K (reprint author), Univ Calif Santa Cruz, UARC, NASA, Ames Res Ctr, MS 269-1, Moffett Field, CA 94035 USA. EM Kamalika.Das@nasa.gov NR 29 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-1864 EI 1932-1872 J9 STAT ANAL DATA MIN JI Stat. Anal. Data Min. PD JUN PY 2013 VL 6 IS 3 SI SI BP 205 EP 220 DI 10.1002/sam.11189 PG 16 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Statistics & Probability SC Computer Science; Mathematics GA V41CW UT WOS:000209525300005 ER PT J AU El Ghaoui, L Pham, V Li, GC Duong, VA Srivastava, A Bhaduri, K AF El Ghaoui, Laurent Vu Pham Li, Guan-Cheng Viet-An Duong Srivastava, Ashok Bhaduri, Kanishka TI Understanding Large Text Corpora via Sparse Machine Learning SO STATISTICAL ANALYSIS AND DATA MINING LA English DT Article DE data mining; intelligent text understanding; sparse machine learning; optimization AB Sparse machine learning has recently emerged as powerful tool to obtain models of high-dimensional data with high degree of interpretability, at low computational cost. The approach has been successfully used in many areas, such as signal and image processing. This article posits that these methods can be extremely useful in the analysis of large collections of text documents, without requiring user expertise in machine learning. Our approach relies on three main ingredients: (i) multidocument text summarization; (ii) comparative summarization of two corpora, both using sparse regression or classification; (iii) sparse principal components and sparse graphical models for unsupervised analysis and visualization of large text corpora. We validate our methods using a corpus of Aviation Safety Reporting System (ASRS) reports and demonstrate that the methods can reveal causal and contributing factors in runway incursions. Furthermore, we show that the methods automatically discover four main tasks that pilots perform during flight, which can aid in further understanding the causal and contributing factors to runway incursions and other drivers for aviation safety incidents. We also provide a comparative study involving other commonly used datasets, and report on the competitiveness of sparse machine learning compared to state-of-the-art methods such as latent Dirichlet allocation (LDA). (c) 2013 Wiley Periodicals, Inc. C1 [El Ghaoui, Laurent; Vu Pham; Li, Guan-Cheng] Univ Calif Berkeley, EECS Dept, Berkeley, CA 94720 USA. [Viet-An Duong] Ecole Mines Ales, Sch Prod & Syst Engn, Ales, France. [Srivastava, Ashok] NASA, Syst Wide Safety & Assurance Technol Project, Moffett Field, CA USA. [Bhaduri, Kanishka] Netflix Inc, Los Gatos, CA USA. RP El Ghaoui, L (reprint author), Univ Calif Berkeley, EECS Dept, Berkeley, CA 94720 USA. EM elghaoui@berkeley.edu NR 55 TC 1 Z9 1 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-1864 EI 1932-1872 J9 STAT ANAL DATA MIN JI Stat. Anal. Data Min. PD JUN PY 2013 VL 6 IS 3 SI SI BP 221 EP 242 DI 10.1002/sam.11187 PG 22 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Statistics & Probability SC Computer Science; Mathematics GA V41CW UT WOS:000209525300006 ER PT J AU Marshall-Bowman, K Barratt, MR Gibson, CR AF Marshall-Bowman, Karina Barratt, Michael R. Gibson, C. Robert TI Ophthalmic changes and increased intracranial pressure associated with long duration spaceflight: An emerging understanding SO ACTA ASTRONAUTICA LA English DT Article DE Vision changes; Microgravity; Long duration spaceflight; Intracranial pressure; Optic disc edema; Visual acuity; Retinal imaging; Optical coherence tomography ID CENTRAL VENOUS-PRESSURE; INTRAOCULAR-PRESSURE; PSEUDOTUMOR CEREBRI; MOUNTAIN-SICKNESS; CHOROIDAL FOLDS; MICROGRAVITY; HYPERTENSION; SPACE; AUTOREGULATION; TRANSIENT AB For many years, there have been anecdotal reports of vision changes by astronauts following short and long-duration spaceflight. Much of this was attributed to hyperopic shifts related to the age of the flying population. However, it has recently been recognized that vision changes are actually quite common in astronauts and are associated with a constellation of findings including elevated intracranial pressure, optic disc edema, globe flattening, optic nerve sheath thickening, hyperopic shifts and retinal changes. With advanced imaging modalities available on the ground along with the fidelity of in-flight diagnostic capabilities previously unavailable, information on this newly recognized syndrome is accumulating. As of this writing, 11 cases of visual impairment experienced by astronauts during missions on-board the International Space Station (ISS) have been documented and studied. Although the exact mechanisms of the vision changes are unknown, it is hypothesized that increased intracranial pressure (ICP) is a contributing factor. Microgravity is the dominant cause of many physiological changes during spaceflight and is thought to contribute significantly to the observed ophthalmic changes. However, several secondary factors that could contribute to increased ICP and vision changes in spaceflight have been proposed. Possible contributors include microgravity-induced cephalad fluid shift, venous obstruction due to microgravity-induced anatomical shifts, high levels of spacecraft cabin carbon dioxide, heavy resistive exercise, and high sodium diet. Individual susceptibility to visual impairment is not fully understood, though a demographic of affected astronauts is emerging. This paper describes the current understanding of this newly recognized syndrome, presents data from 11 individual cases, and discusses details of potential contributing factors. The occurrence of visual changes in long duration missions in microgravity is one of the most significant clinical issues to date for the human spaceflight community, and a comprehensive understanding of the issue at whole is critical to ensure safe space exploration in the future. (C) 2013 Published by Elsevier Ltd. on behalf of IAA. C1 [Marshall-Bowman, Karina; Barratt, Michael R.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Marshall-Bowman, Karina] German Aerosp Ctr DLR, Inst Aerosp Med, D-51147 Cologne, Germany. [Gibson, C. Robert] Wyle Sci Technol & Engn, Houston, TX USA. RP Barratt, MR (reprint author), NASA, Lyndon B Johnson Space Ctr, CB, Astronaut Off, 2101 NASA Pkwy, Houston, TX 77058 USA. EM Karina.Marshall-Bowman@dlr.de; Michael.r.barratt@nasa.gov; charles.gibson-1@nasa.gov OI Marshall-Goebel, Karina/0000-0002-5240-7625 NR 43 TC 11 Z9 12 U1 3 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN-JUL PY 2013 VL 87 BP 77 EP 87 DI 10.1016/j.actaastro.2013.01.014 PG 11 WC Engineering, Aerospace SC Engineering GA 133IE UT WOS:000318131300008 ER PT J AU Grintzalis, K Zisimopoulos, D Grune, T Weber, D Georgiou, CD AF Grintzalis, Konstantinos Zisimopoulos, Dimitrios Grune, Tilman Weber, Daniela Georgiou, Christos D. TI Method for the simultaneous determination of free/protein malondialdehyde and lipid/protein hydroperoxides SO FREE RADICAL BIOLOGY AND MEDICINE LA English DT Article DE Lipid/protein malondialdehyde; Thiobarbituric acid; Lipid/protein hydroperoxides; Oxidative stress; Xylenol orange; Free radicals ID LOW-DENSITY-LIPOPROTEIN; XYLENOL ORANGE ASSAY; 4-HYDROXYNONENAL MODIFIED PROTEINS; LIPID-PEROXIDATION PRODUCTS; FERROUS ION OXIDATION; THIOBARBITURIC ACID; AMINO-ACID; IMMUNOCHEMICAL DETECTION; BIOLOGICAL SAMPLES; HYDROGEN-PEROXIDE AB A simple and sensitive method is presented for the simultaneous quantification (spectrophotometric and spectrofluorimetric) of the main lipid and protein peroxidation products after their initial fractionation: free malondialdehyde (FrMDA), protein-bound malondialdehyde (PrMDA), total hydroperoxides (LOON), and protein hydroperoxides (PrOOH). FrMDA and PrMDA (released from proteins by alkaline hydrolysis) are measured after the reaction of MDA with thiobarbituric acid (TBA) under acidic conditions, by the specific fluorimetric quantification of the resulting MDA-(TBA)(2) adduct chromophore. The measurement of LOOH and PrOOH is based on the reaction of Fe3+ (resulting from the reaction of LOOH and PrOOH with Fe2+) with xylenol orange (XO) and the, photometric quantification of the resulting XO-Fe complex. The sensitivity of the assays for FrMDA/PrMDA and LOOH/PrOOH is 20 and 100 pmol respectively. The method was applied successfully on human plasma and can be used. for the evaluation of oxidative stress in both basic and clinical research. (c) 2012 Elsevier Inc. All rights reserved. C1 [Grintzalis, Konstantinos; Zisimopoulos, Dimitrios; Georgiou, Christos D.] Univ Patras, Dept Biol, Genet Cell & Dev Biol Sect, Patras 26100, Greece. [Grune, Tilman; Weber, Daniela] Univ Jena, Dept Nutr Toxicol, Inst Nutr, Jena, Germany. [Georgiou, Christos D.] NASA, ARC, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Georgiou, CD (reprint author), Univ Patras, Dept Biol, Cell & Dev Biol Sect, Patras 26100, Greece. EM c.georgiou@upatras.gr RI Georgiou, Christos/B-8354-2013; Grintzalis, Konstantinos/I-5124-2014; OI Georgiou, Christos/0000-0001-9707-0109; Grintzalis, Konstantinos/0000-0002-6276-495X; Grune, Tilman/0000-0003-4775-9973; Weber, Daniela/0000-0002-2054-6233 FU Greek Ministry of Education, University of Patras, Greece FX This work was financially supported by the Greek Ministry of Education, University of Patras, Greece. The authors express their gratitude to Dr. Janusz (Jan) Gebicki (Department of Biological Sciences, Macquarie University, Australia) for his very useful suggestions. NR 60 TC 13 Z9 13 U1 4 U2 44 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0891-5849 J9 FREE RADICAL BIO MED JI Free Radic. Biol. Med. PD JUN PY 2013 VL 59 BP 27 EP 35 DI 10.1016/j.freeradbiomed.2012.09.038 PG 9 WC Biochemistry & Molecular Biology; Endocrinology & Metabolism SC Biochemistry & Molecular Biology; Endocrinology & Metabolism GA 134IE UT WOS:000318202800004 PM 23041350 ER PT J AU Konishi, C Mudawar, I Hasan, MM AF Konishi, Christopher Mudawar, Issam Hasan, Mohammad M. TI Investigation of the influence of orientation on critical heat flux for flow boiling with two-phase inlet SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Flow boiling; Critical heat flux; Flow orientation ID RECTANGULAR IMPINGING JET; DIELECTRIC LIQUID; VERTICAL SURFACES; CHF MECHANISM; SINGLE-PHASE; BODY FORCE; CHANNEL; MODEL; MICROGRAVITY; DISCRETE AB This study explores the mechanism of flow boiling critical heat flux (CHF) for FC-72 in a rectangular channel fitted along one side with a heated wall. The flow is supplied as a two-phase mixture and the channel is tested at different orientations relative to Earth's gravity. High-speed video imaging is used to identify the CHF trigger mechanism for different orientations, mass velocities and inlet qualities. It is shown that orientation has a significant influence on CHF for low mass velocities and small inlet qualities, with the orientations surrounding horizontal flow with downward-facing heated wall causing stratification of the vapor towards the heated wall and yielding very small CHF values. High mass velocities cause appreciable diminution in the influence of orientation on CHF, which is evidenced by similar flow patterns and CHF trigger mechanism regardless of orientation. The interfacial lift-off model is shown to predict the influence of orientation on CHF with good accuracy. Overall, this study points to the effectiveness of high mass velocities at combating buoyancy effects and helping produce CHF values insensitive to orientation. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Konishi, Christopher; Mudawar, Issam] Purdue Univ, Sch Mech Engn, BTPFL, W Lafayette, IN 47907 USA. [Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mudawar, I (reprint author), Purdue Univ, Sch Mech Engn, BTPFL, 585 Purdue Mall, W Lafayette, IN 47907 USA. EM mudawar@ecn.purdue.edu FU National Aeronautics and Space Administration (NASA) [NNX12AK14G] FX The authors are grateful for the support of this project by the National Aeronautics and Space Administration (NASA) under grant no. NNX12AK14G. NR 38 TC 12 Z9 13 U1 1 U2 16 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 JUN PY 2013 VL 61 BP 176 EP 190 DI 10.1016/j.ijheatmasstransfer.2013.01.076 PG 15 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 135BE UT WOS:000318260200019 ER PT J AU Lee, H Mudawar, I Hasan, MM AF Lee, Hyoungsoon Mudawar, Issam Hasan, Mohammad M. TI Experimental and theoretical investigation of annular flow condensation in microgravity SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Microgravity; Condensation; Annular flow ID CRITICAL HEAT-FLUX; FALLING LIQUID-FILMS; TRANSFER COEFFICIENT; PRESSURE-DROP; BOILING CHF; MOMENTUM TRANSPORT; UNIVERSAL APPROACH; SINGLE-PHASE; BODY FORCE; TUBES AB Vehicles for future manned space missions will demand unprecedented increases in power requirements and heat dissipation. Achieving these goals while maintaining acceptable size and weight limits will require replacing present single-phase thermal management components with far more efficient two-phase counterparts. This study discusses the development of an experimental facility for the study of annular condensation of FC-72 in microgravity, which was tested in parabolic flight as a prelude to the development of NASA's Flow Boiling and Condensation Experiment (FBCE) for the International Space Station (ISS). The flow behavior of the condensate film is shown to be sensitive mostly to the mass velocity of FC-72, with low mass velocities yielding laminar flow with a smooth interface, and high mass velocities turbulent flow with appreciable interfacial waviness. A select number of tests repeated in microgravity, Lunar gravity and Martian gravity prove that the influence of gravity is very pronounced at low mass velocities, manifest by circumferential uniformity for microgravity versus appreciable thickening along one side of the condensation tube for Lunar and Martian conditions. However, the thickening is nonexistent for Lunar and Martian conditions at high mass velocities due to increased vapor shear on the film interface, proving high mass velocity is an effective means to negating the influence of gravity in space missions. For microgravity, the condensation heat transfer coefficient is highest near the inlet, where the film is both thin and laminar, and decreases along the condensation length, but increases again downstream for high mass velocities due to turbulence and increased waviness. A model is proposed to predict the condensation heat transfer which accounts for dampening of turbulent fluctuations near the film interface. The model shows good agreement with the heat transfer coefficient data in both trend and magnitude. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Lee, Hyoungsoon; Mudawar, Issam] Purdue Univ, Boiling & Two Phase Flow Lab, Sch Mech Engn, W Lafayette, IN 47907 USA. [Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mudawar, I (reprint author), Purdue Univ, Boiling & Two Phase Flow Lab, Sch Mech Engn, 585 Purdue Mall, W Lafayette, IN 47907 USA. EM mudawar@ecn.purdue.edu FU National Aeronautics and Space Administration (NASA) [NNX13AB01G] FX The authors are grateful for the support of the National Aeronautics and Space Administration (NASA) under grant no. NNX13AB01G. The authors thank Rochelle May, Jeffrey Juergens, James Wagner, Nancy Hall, Henry Nahra, David Chao, Robert Butcher, Alban Seigneur, Bruce Frankenfield, Paul Trimarchi, Richard Kelsch, Daniel Gotti, Chip Redding, and Frank Kmiecik of the NASA Glenn Research Center, and Jeffrey Mackey of Vantage Partners LLC for their technical assistance. NR 54 TC 15 Z9 16 U1 6 U2 40 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 JUN PY 2013 VL 61 BP 293 EP 309 DI 10.1016/j.ijheatmasstransfer.2013.02.010 PG 17 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 135BE UT WOS:000318260200029 ER PT J AU Miller, JE Bohl, WE Christiansen, EL Davis, BA AF Miller, J. E. Bohl, W. E. Christiansen, E. L. Davis, B. A. TI Ballistic performance of porous-ceramic, thermal protection systems SO INTERNATIONAL JOURNAL OF IMPACT ENGINEERING LA English DT Article; Proceedings Paper CT 12th Hypervelocity Impact Symposium (HVIS) CY SEP 16-20, 2012 CL Baltimore, MD DE MMOD; TPS; Tile; Ballistic performance AB Porous-ceramic, thermal protection systems were used heavily on the Orbiter, and they are currently being used on the next generation of US manned spacecraft, Orion. These systems insulate reentry critical components of a spacecraft against the intense thermal environments of atmospheric reentry. Additionally, these materials are highly exposed to space environment hazards like solid particle impacts. This paper discusses impact studies up to 10 km/s on nominally 8 lb/ft(3) alumina-fiber-enhanced-thermal-barrier (AETB8) tiles coated with a toughened-unipiece-fibrous-insulation/reaction-cured-glass layer (TUFI/RCG). A first principles impact model that describes projectile dispersion is described that provides excellent agreement with observations over a broad range of impact velocities, obliquities and projectile materials. 2012 Published by Elsevier Ltd. Selection and/or peer-review under responsibility of the International Hypervelocity Impact Society. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Miller, J. E.; Bohl, W. E.] Lockheed Martin Space Syst Co, Denver, CO 80127 USA. [Christiansen, E. L.; Davis, B. A.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Miller, JE (reprint author), Lockheed Martin Space Syst Co, Denver, CO 80127 USA. EM joshua.e.miller@lmco.com NR 9 TC 6 Z9 6 U1 5 U2 44 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0734-743X J9 INT J IMPACT ENG JI Int. J. Impact Eng. PD JUN PY 2013 VL 56 SI SI BP 40 EP 46 DI 10.1016/j.ijimpeng.2012.07.005 PG 7 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 131LG UT WOS:000317994600008 ER PT J AU Semiatin, SL McClary, KE Rollett, AD Roberts, CG Payton, EJ Zhang, F Gabb, TP AF Semiatin, S. L. McClary, K. E. Rollett, A. D. Roberts, C. G. Payton, E. J. Zhang, F. Gabb, T. P. TI Plastic Flow and Microstructure Evolution during Thermomechanical Processing of a PM Nickel-Base Superalloy SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID ISOTHERMAL FORGING CONDITIONS; ABNORMAL GRAIN-GROWTH; DEFORMATION; COMPRESSION; ALLOYS AB Plastic flow and microstructure evolution during sub- and supersolvus forging and subsequent supersolvus heat treatment of the powder-metallurgy superalloy LSHR (low-solvus, high-refractory) were investigated to develop an understanding of methods that can be used to obtain a moderately coarse gamma grain size under well-controlled conditions. To this end, isothermal, hot compression tests were conducted over broad ranges of temperature [(1144 K to 1450 K) 871 A degrees C to 1177 A degrees C] and constant true strain rate (0.0005 to 10 s(-1)). At low temperatures, deformation was generally characterized by flow softening and dynamic recrystallization that led to a decrease in grain size. At high subsolvus temperatures and low strain rates, steady-state flow or flow hardening was observed. These latter behaviors were ascribed to superplastic deformation and microstructure evolution characterized by a constant grain size or concomitant dynamic grain growth, respectively. During supersolvus heat treatment following subsolvus deformation, increases in grain size whose magnitude was a function of the prior deformation conditions were noted. A transition in flow behavior from superplastic to nonsuperplastic and the development during forging at a high subsolvus temperature of a wide (possibly bi- or multimodal) gamma-grain-size distribution having some large grains led to a substantially coarser grain size during supersolvus annealing in comparison to that produced under all other forging conditions. C1 [Semiatin, S. L.] USAF, Res Lab, Mat & Mfg Directorate, AFRL RXCM, Wright Patterson AFB, OH 45433 USA. [McClary, K. E.] Wright State Univ, Dept Phys, Dayton, OH 45435 USA. [Rollett, A. D.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA. [Roberts, C. G.] Vallourec & Mannesmann USA Corp, Youngstown, OH 44510 USA. [Payton, E. J.] BAM Fed Inst Mat Res & Testing, D-12205 Berlin, Germany. [Zhang, F.] Computherm LLC, Madison, WI 53719 USA. [Gabb, T. P.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Semiatin, SL (reprint author), USAF, Res Lab, Mat & Mfg Directorate, AFRL RXCM, Wright Patterson AFB, OH 45433 USA. EM Lee.Semiatin@wpafb.af.mil RI Rollett, Anthony/A-4096-2012; SEMIATIN, SHELDON/E-7264-2017; OI Rollett, Anthony/0000-0003-4445-2191; Payton, Eric/0000-0001-7478-9372 FU Air Force STW-21 Initiative [F33615-01-2-5225]; MRSEC at Carnegie Mellon University, NSF [DMR-0520425] FX This work was conducted as part of the in-house research of the Metals Branch of the Air Force Research Laboratory's Materials and Manufacturing Directorate. The support and encouragement of the Laboratory management are gratefully acknowledged. The assistance of P.N. Fagin and T. M. Brown in conducting the experiments and A. Shively, A. L. Pilchak, and A. A. Salem in segmenting EBSD/EDS data is greatly appreciated. Technical discussions with P. L. Martin (AFRL) and J. Gayda and J. Telesman (NASA GRC) are also much appreciated. Two of the authors (ADR and CGR) also acknowledge support from the Air Force STW-21 Initiative, Contract F33615-01-2-5225, and the MRSEC at Carnegie Mellon University, NSF Grant Number DMR-0520425. NR 34 TC 17 Z9 17 U1 5 U2 38 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD JUN PY 2013 VL 44A IS 6 BP 2778 EP 2798 DI 10.1007/s11661-013-1675-1 PG 21 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 130PI UT WOS:000317930200032 ER PT J AU Calle, CI Mackey, PJ Hogue, MD Johansen, MR Kelley, JD Phillips, JR Clements, JS AF Calle, C. I. Mackey, P. J. Hogue, M. D. Johansen, M. R. Kelley, J. D. Phillips, J. R., III Clements, J. S. TI An electrostatic precipitator system for the Martian environment SO JOURNAL OF ELECTROSTATICS LA English DT Article DE Space applications; Electrostatic precipitator; Particle control; Particle charging AB Human exploration missions to Mars will require the development of technologies for the utilization of the planet's own resources for the production of commodities. However, the Martian atmosphere contains large amounts of dust. The extraction of commodities from this atmosphere requires prior removal of this dust. We report on our development of an electrostatic precipitator able to collect Martian simulated dust particles in atmospheric conditions approaching those of Mars. Extensive experiments with an initial prototype in a simulated Martian atmosphere showed efficiencies of 99%. The design of a second prototype with aerosolized Martian simulated dust in a flow-through is described. Published by Elsevier B.V. C1 [Calle, C. I.; Mackey, P. J.; Hogue, M. D.; Johansen, M. R.] NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. [Kelley, J. D.; Phillips, J. R., III; Clements, J. S.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. RP Calle, CI (reprint author), NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. EM carlos.i.calle@nasa.gov NR 5 TC 1 Z9 1 U1 2 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3886 J9 J ELECTROSTAT JI J. Electrost. PD JUN PY 2013 VL 71 IS 3 BP 254 EP 256 DI 10.1016/j.elstat.2012.10.008 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 128WI UT WOS:000317800000015 ER PT J AU Calle, CI Mackey, PJ Hogue, MD Johansen, MR Yim, H Delaune, PB Clements, JS AF Calle, C. I. Mackey, P. J. Hogue, M. D. Johansen, M. R. Yim, H. Delaune, P. B. Clements, J. S. TI Electrodynamic Dust Shields on the International Space Station: Exposure to the space environment SO JOURNAL OF ELECTROSTATICS LA English DT Article DE Space applications; Particle control; Particle charging AB Electrodynamic Dust Shields (EDS) have been in development at NASA as a dust mitigation method for lunar and Martian missions. An active dust mitigation strategy, such as that provided by the EDS, that can remove dust from surfaces, is of crucial importance to the planetary exploration program. We report on the development of a flight experiment to fully expose four EDS panels to the space environment. This flight experiment is part of the Materials International Space Station experiment X (MISSE-X), an external platform on the International Space Station that will expose materials to the space environment. (C) 2012 Published by Elsevier B.V. C1 [Calle, C. I.; Mackey, P. J.; Hogue, M. D.; Johansen, M. R.] NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. [Yim, H.; Delaune, P. B.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Clements, J. S.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. RP Calle, CI (reprint author), NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. EM Carlos.I.Calle@nasa.gov NR 6 TC 0 Z9 0 U1 2 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3886 J9 J ELECTROSTAT JI J. Electrost. PD JUN PY 2013 VL 71 IS 3 BP 257 EP 259 DI 10.1016/j.elstat.2012.10.009 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 128WI UT WOS:000317800000016 ER PT J AU Farley, KA Hurowitz, JA Asimow, PD Jacobson, NS Cartwright, JA AF Farley, K. A. Hurowitz, J. A. Asimow, P. D. Jacobson, N. S. Cartwright, J. A. TI A double-spike method for K-Ar measurement: A technique for high precision in situ dating on Mars and other planetary surfaces SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID MASS-SPECTROMETRY; HIGH-TEMPERATURE; CROSS-SECTIONS; AGES; IONIZATION; CHRONOLOGY; EVOLUTION; HISTORY; ZAGAMI; PB AB A new method for K-Ar dating using a double isotope dilution technique is proposed and demonstrated. The method is designed to eliminate known difficulties facing in situ dating on planetary surfaces, especially instrument complexity and power availability. It may also have applicability in some terrestrial dating applications. Key to the method is the use of a solid tracer spike enriched in both Ar-39 and K-41. When mixed with lithium borate flux in a Knudsen effusion cell, this tracer spike and a sample to be dated can be successfully fused and degassed of Ar at <1000 degrees C. The evolved Ar-40*/Ar-39 ratio can be measured to high precision using noble gas mass spectrometry. After argon measurement the sample melt is heated to a slightly higher temperature (similar to 1030 degrees C) to volatilize potassium, and the evolved K-39/K-41 ratio measured by Knudsen effusion mass spectrometry. Combined with the known composition of the tracer spike, these two ratios define the K-Ar age using a single sample aliquot and without the need for extreme temperature or a mass determination. In principle the method can be implemented using a single mass spectrometer. Experiments indicate that quantitative extraction of argon from a basalt sample occurs at a sufficiently low temperature that potassium loss in this step is unimportant. Similarly, potassium isotope ratios measured in the Knudsen apparatus indicate good sample-spike equilibration and acceptably small isotopic fractionation. When applied to a flood basalt from the Viluy Traps, Siberia, a K-Ar age of 351 +/- 19 Ma was obtained, a result within 1% of the independently known age. For practical reasons this measurement was made on two separate mass spectrometers, but a scheme for combining the measurements in a single analytical instrument is described. Because both parent and daughter are determined by isotope dilution, the precision on K-Ar ages obtained by the double isotope dilution method should routinely approach that of a pair of isotope ratio determinations, likely better than +/- 5%. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Farley, K. A.; Asimow, P. D.; Cartwright, J. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Hurowitz, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jacobson, N. S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Farley, KA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM farley@gps.caltech.edu RI Cartwright, Julia/A-8470-2013 FU Keck Institute for Space Studies; National Aeronautics and Space Agency (JAH) FX We thank Paul Renne for suggesting and providing the Viluy Traps basalt sample and Tim Becker for facilitating the irradiation of our spike glass. We thank Leah Morgan, Pete Burnard, and two anonymous reviewers for helpful suggestions. This work could not have occurred without the generous and patient support of the Keck Institute for Space Studies. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Agency (JAH). NR 34 TC 10 Z9 10 U1 2 U2 41 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 JUN 1 PY 2013 VL 110 BP 1 EP 12 DI 10.1016/j.gca.2013.02.010 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 123IH UT WOS:000317381100001 ER PT J AU Vance, S Brown, JM AF Vance, Steve Brown, J. Michael TI Thermodynamic properties of aqueous MgSO4 to 800 MPa at temperatures from-20 to 100 degrees C and concentrations to 2.5 mol kg(-1) from sound speeds, with applications to icy world oceans SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID DIAMOND-ANVIL CELL; LINEAR ISOPIESTIC RELATION; EQUATION-OF-STATE; MAJOR SEA SALTS; MAGNESIUM-SULFATE; PVT PROPERTIES; INTERNAL STRUCTURE; SUBSURFACE OCEANS; WATER; APPARENT AB Thermodynamic properties of aqueous magnesium sulfate solutions (MgSO4 concentrations to 2.5 mol kg(-1)) are reported in a previously unexplored regime of pressure and temperature. Solution densities (to a few hundred parts-per-million), specifics heats (to a few percent), and volumetric mixing parameters were determined to 800 MPa in the temperature range from -20 to 100 degrees C from sound speeds measurements. Equilibrium data extrapolate smoothly to temperatures below which liquids are stable, providing a basis for equilibrium freezing calculations. In more compressed water at high pressure, where electrostrictive effects are smaller, the partial molal volume at infinite dilution is positive and changes less with pressure, while the non-ideal contribution to the apparent molal volume is reduced. Ion-solvent and ion-ion contributions are small under all conditions, while solvent contributions to non-ideality show greater variation with pressure and temperature. In application to Ganymede, Callisto, and Titan, the current results suggest that concentrations of aqueous MgSO4 would be exist that would be denser than overlying ice and thus buoyantly stable at the ice VI-rock interface, or between overlying layers of ice VI-V or V-III. More generally, the current data and analysis provide a comprehensive framework that can guide investigations of other single and multi-component aqueous systems. (C) 2013 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Univ Washington, Seattle, WA 98195 USA. RP Vance, S (reprint author), MS 183-401,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM svance@jpl.nasa.gov FU NASA [NNG06GF81G, NNX08AQ51G, 08-NAI5-0021]; National Science Foundation's IGERT program [DGE-9870713] FX This work was partially supported by NASA Outer Planets Research through grants NNG06GF81G and NNX08AQ51G, by the National Science Foundation's IGERT program, grant number DGE-9870713, "IGERT: Astrobiology: Life in and beyond Earth's Solar System," by the Icy Worlds node of NASA's Astrobiology Institute (08-NAI5-0021) and the NASA and Caltech postdoctoral programs. Laboratory efforts benefited from substantial work by Evan Abramson, Nicholas Castle, Steven Domonkos, Kyle Straughn, and Hoku West-Foyle. Discussions with Evan Abramson are acknowledged and appreciated. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Copyright statement must be added until copyright is transferred to publisher. NR 63 TC 8 Z9 8 U1 1 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 JUN 1 PY 2013 VL 110 BP 176 EP 189 DI 10.1016/j.gca.2013.01.040 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 123IH UT WOS:000317381100011 ER PT J AU Craig, L Moharreri, A Schanot, A Rogers, DC Anderson, B Dhaniyala, S AF Craig, Lucas Moharreri, Arash Schanot, Allen Rogers, David C. Anderson, Bruce Dhaniyala, Suresh TI Characterizations of Cloud Droplet Shatter Artifacts in Two Airborne Aerosol Inlets SO AEROSOL SCIENCE AND TECHNOLOGY LA English DT Article ID SINGLE DROP; CONDENSATION NUCLEI; SOLID-SURFACES; IMPACT; DEFORMATION; BREAKUP; PERFORMANCE; PARTICLES AB Aircraft-based aerosol sampling in clouds is complicated by the generation of shatter artifact particles from aerodynamic or impaction breakup of cloud droplets and ice particles in and around the aerosol inlet. Aerodynamic breakup occurs when the Weber number of a droplet, which primarily depends on the droplet size and the magnitude of the relative motion of the droplet and the local air mass, exceeds a critical value. Impaction breakup of a droplet occurs when the droplet's impaction breakup parameter, K, which is a combination of Weber and Ohnesorge numbers, exceeds a critical value. Considering these two mechanisms, the critical breakup diameters are estimated for two aerosol inlets of different designsa conventional forward-facing solid diffuser inlet (SDI) and a cross-flow sampling sub-micron aerosol inlet (SMAI). From numerical simulations, it is determined that cloud droplets of all sizes will experience impaction breakup in SDI, while only droplets larger than approximate to 16m will experience impaction breakup in SMAI. The relatively better in-cloud sampling performance of SMAI is because of its cone design that slows the flow just upstream of the sample tube. The slowing upstream flow, however, causes aerodynamic breakup of drops larger than approximate to 100m. The critical breakup diameters determined from analysis of field data largely validate numerical predictions. The cross-flow sampling design of SMAI is seen to ensure that shatter artifacts in the inlet are minimal even when there are a significant number of particles larger that the critical breakup size. The study results, thus, suggest that the SMAI design presents an effective approach to sample interstitial particles from aircraft. Copyright 2013 American Association for Aerosol Research C1 [Craig, Lucas; Moharreri, Arash; Dhaniyala, Suresh] Clarkson Univ, Dept Mech & Aeronaut Engn, Potsdam, NY 13699 USA. [Schanot, Allen; Rogers, David C.] NCAR RAF, Earth Observing Lab, Broomfield, CO USA. [Anderson, Bruce] NASA LaRC, Chem & Dynam Branch, Langley, VA USA. RP Dhaniyala, S (reprint author), Clarkson Univ, Dept Mech & Aeronaut Engn, 8 Clarkson Ave, Potsdam, NY 13699 USA. EM sdhaniyala@clarkson.edu FU NASA (GSRP) [NNX09AJ08H]; NSF [AGS-1044989, AGS-1121915] FX The authors acknowledge funding support from NASA's Graduate Student Research Fellowship (GSRP; Cooperative agreement number: NNX09AJ08H) and NSF (AGS-1044989 and AGS-1121915). We would also like to thank Antony Clarke for the SDI data. NR 43 TC 6 Z9 6 U1 0 U2 14 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0278-6826 J9 AEROSOL SCI TECH JI Aerosol Sci. Technol. PD JUN 1 PY 2013 VL 47 IS 6 BP 662 EP 671 DI 10.1080/02786826.2013.780648 PG 10 WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 122BQ UT WOS:000317290600009 ER PT J AU Lourie, NP Chuss, DT Henry, RM Wollack, EJ AF Lourie, Nathan P. Chuss, David T. Henry, Ross M. Wollack, Edward J. TI Investigation of truncated waveguides SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS LA English DT Article DE circuit synthesis and modeling; polarization; waveguide components; eigenvalue calculation ID WAVELENGTHS AB The design, fabrication, and performance of truncated circular and square waveguide cross-sections are presented. An emphasis is placed upon numerical and experimental validation of simple analytical formulae that describe the propagation properties of these structures. A test component, a 90-degree phase shifter, was fabricated and tested at 30 GHz. The concepts explored can be directly applied in the design, synthesis and optimization of components in the microwave to submillimeter wavebands. (c) 2013 Wiley Periodicals, Inc. Microwave Opt Technol Lett 55:12811285, 2013; View this article online at wileyonlinelibrary.com. DOI 10.1002/mop.27561 C1 [Lourie, Nathan P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Chuss, David T.; Henry, Ross M.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Chuss, DT (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. EM David.T.Chuss@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 NR 24 TC 0 Z9 0 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0895-2477 J9 MICROW OPT TECHN LET JI Microw. Opt. Technol. Lett. PD JUN PY 2013 VL 55 IS 6 BP 1281 EP 1285 DI 10.1002/mop.27561 PG 5 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA 117PW UT WOS:000316966600025 ER PT J AU Finley, AO Banerjee, S Cook, BD Bradford, JB AF Finley, Andrew O. Banerjee, Sudipto Cook, Bruce D. Bradford, John B. TI Hierarchical Bayesian spatial models for predicting multiple forest variables using waveform LiDAR, hyperspectral imagery, and large inventory datasets SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION LA English DT Article DE LiDAR; Hyperspectral; Bayesian hierarchical spatial models; Gaussian Predictive process; Forestry ID DATA SETS; LIKELIHOOD AB In this paper we detail a multivariate spatial regression model that couples LiDAR, hyperspectral and forest inventory data to predict forest outcome variables at a high spatial resolution. The proposed model is used to analyze forest inventory data collected on the US Forest Service Penobscot Experimental Forest (PEF), ME, USA. In addition to helping meet the regression model's assumptions, results from the PEF analysis suggest that the addition of multivariate spatial random effects improves model fit and predictive ability, compared with two commonly applied modeling approaches. This improvement results from explicitly modeling the covariation among forest outcome variables and spatial dependence among observations through the random effects. Direct application of such multivariate models to even moderately large datasets is often computationally infeasible because of cubic order matrix algorithms involved in estimation. We apply a spatial dimension reduction technique to help overcome this computational hurdle without sacrificing richness in modeling. (C) 2012 Elsevier B.V. All rights reserved. C1 [Finley, Andrew O.] Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. [Finley, Andrew O.] Michigan State Univ, Dept Geog, E Lansing, MI 48824 USA. [Banerjee, Sudipto] Univ Minnesota, Div Biostat, Minneapolis, MN USA. [Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Bradford, John B.] US Geol Survey, Southwest Biol Sci Ctr, Flagstaff, AZ 86001 USA. RP Finley, AO (reprint author), Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. EM finleya@msu.edu RI Bradford, John/E-5545-2011; Cook, Bruce/M-4828-2013; Beckley, Matthew/D-4547-2013 OI Cook, Bruce/0000-0002-8528-000X; FU USDA Forest Service; Forest Inventory and Analysis National Program; Forest Health Technology Enterprise Team; National Science Foundation (NSF) [EF-1137309]; USDA/NASA grant [10-JV-11242307037]; U.S. Forest Service; [NSF-DMS-1106609] FX The work of the first author was supported by the USDA Forest Service, Forest Inventory and Analysis National Program, Forest Health Technology Enterprise Team, and National Science Foundation (NSF) grant EF-1137309. The first and second authors were supported by the grant NSF-DMS-1106609. The first and fourth authors were supported by USDA/NASA grant 10-JV-11242307-037.; Data for this study were provided by a unit of the Northern Research Station, U.S. Forest Service, located at the Penobscot Experimental Forest in Maine. Significant funding for collection of these data was provided by the U.S. Forest Service. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 48 TC 6 Z9 6 U1 2 U2 36 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0303-2434 J9 INT J APPL EARTH OBS JI Int. J. Appl. Earth Obs. Geoinf. PD JUN PY 2013 VL 22 SI SI BP 147 EP 160 DI 10.1016/j.jag.2012.04.007 PG 14 WC Remote Sensing SC Remote Sensing GA 111NU UT WOS:000316528800015 ER PT J AU Akamatsu, H Gottardi, L Adams, J Bailey, C Bandler, S Bruijn, M Chervenak, J Eckart, M Finkbeiner, F den Hartog, R Hoevers, H Kelley, R van der Kuur, J van den Linden, T Lindeman, M Porter, F Sadleir, J Smith, S Beyer, J Kiviranta, M AF Akamatsu, H. Gottardi, L. Adams, J. Bailey, C. Bandler, S. Bruijn, M. Chervenak, J. Eckart, M. Finkbeiner, F. den Hartog, R. Hoevers, H. Kelley, R. van der Kuur, J. van den Linden, T. Lindeman, M. Porter, F. Sadleir, J. Smith, S. Beyer, J. Kiviranta, M. TI Single Pixel Characterization of X-Ray TES Microcalorimeter Under AC Bias at MHz Frequencies SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Astrophysics; spectroscopy; X-ray detectors ID ABSORBER DESIGN; PERFORMANCE; ARRAYS AB In this paper, we present the progress made at SRON in the read-out of X-ray Transition Edge Sensor (TES) microcalorimeters under AC bias. The experiments reported so far, whose aim was to demonstrate an energy resolution of 2 eV at 6 keV with a TES acting as a modulator, were carried out at frequencies below 700 kHz using a standard flux locked loop SQUID read-out scheme. The TES read-out suffered from the use of suboptimal circuit components, large parasitic inductances, low quality factor resonators, and poor magnetic field shielding. We have developed a novel experimental set-up that allows us to test several read-out schemes in a single cryogenic run. In this set-up, the TES pixels from a GSFC array are coupled via superconducting transformers to 18 high-Q lithographic LC filters with resonant frequencies ranging between 2 and 5 MHz. The signal is amplified by a two-stage SQUID current sensor and baseband feedback is used to overcome the limited SQUID dynamic range. We measured an X-ray energy resolution of 3.6 eV at 1.4 MHz, which is consistent with the measured integrated Noise Equivalent Power. C1 [Akamatsu, H.; Gottardi, L.; Bruijn, M.; den Hartog, R.; Hoevers, H.; van der Kuur, J.; van den Linden, T.; Lindeman, M.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Adams, J.; Bailey, C.; Bandler, S.; Chervenak, J.; Eckart, M.; Finkbeiner, F.; Kelley, R.; Porter, F.; Sadleir, J.; Smith, S.] NASA, Goddard Space Flight Ctr 662, Greenbelt, MD USA. [Beyer, J.] PTB Berlin, Berlin, Germany. [Kiviranta, M.] VTT, Espoo, Finland. RP Akamatsu, H (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM h.akamatsu@sron.nl RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Porter, Frederick/D-3501-2012 OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106; Porter, Frederick/0000-0002-6374-1119 NR 12 TC 4 Z9 4 U1 0 U2 27 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2100503 DI 10.1109/TASC.2012.2235509 PN 1 PG 3 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 080ZM UT WOS:000314283800067 ER PT J AU Beyer, AD Echternach, PM Kenyon, ME Runyan, MC Bumble, B Bradford, CM Bock, JJ Holmes, WA AF Beyer, Andrew D. Echternach, Pierre M. Kenyon, Matthew E. Runyan, Marcus C. Bumble, Bruce Bradford, Charles M. Bock, James J. Holmes, Warren A. TI Effect of Mo/Cu Superconducting Bilayer Geometry on Ultra-Sensitive Transition-Edge Sensor Performance SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Infrared superconducting detectors; proximity effect; sub-mm superconducting detectors; transition edge sensors (TESs) AB We built membrane-isolated transition-edge sensors (TESs) for the background-limited infrared/sub-mm spectrograph using Mo/Cu superconducting bilayer thermistors of varying geometry and found that undesired proximity effects, including the so-called longitudinal proximity effect (LoPE) and the latitudinal inverse proximity effect, affect both the superconducting transition temperature T-C and the sharpness of the transition alpha = d log R/d log T. The LoPE and latitudinal inverse proximity effect arise because of unintentional proximity effects between the bilayer thermistors, the superconducting wiring of the TES circuitry, and normal metal decorations added to mitigate the LoPE. We examined Mo/Cu bilayer films with widths of 120 mu m and lengths of 5, 10, 20, 40, and 120 mu m, and studied the variation of T-C, alpha, and approximate 80% resistance per square (R-0.8) with Ti (T-C similar to 500 mK) and TiN (T-C similar to 3.8 K) wiring to the devices. We found larger a values in general for the Ti wiring, where a was as high as 90 for 20-120 mu m devices and decreased to 20 for 5-mu m-wide devices. We then built arrays of TESs with bilayer thermistor lengths of 10 mu m, Ti contacts, TiN wiring, and Au borders. The devices were expected to demonstrate a noise equivalent power less than or equal to 10(-19) W/Hz(1/2). We report a measured noise equivalent power at 87 mK of (0.95 +/- 0.2) x 10(-19) W/Hz(1/2) and a response time tau of (360 +/- 30)ms on our best device with a thermal conductance G = (15 +/- 5)fW/K, T-C = (120.5 +/- 3.5)mK, and stray power P-D = (135 +/- 85)aW. The thermistor had a value of R-N = 6 m Omega and value of alpha = d log R/d log T between 10 and 60 in the transition. We compare our measured performance with the performance specifications needed for ultrasensitive TESs on the Background-Limited Infrared/Sub-mm Spectrograph (BLISS) and discuss paths forward. C1 [Beyer, Andrew D.; Echternach, Pierre M.; Kenyon, Matthew E.; Runyan, Marcus C.; Bumble, Bruce; Bradford, Charles M.; Bock, James J.; Holmes, Warren A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Beyer, AD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM Andrew.d.beyer@jpl.nasa.gov; Pierre.M.Echternach@jpl.nasa.gov; matthew.e.kenyon@jpl.nasa.gov; mcr@caltech.edu; Bruce.Bumble@jpl.nasa.gov; bradford@submm.caltech.edu; jjb@astro.caltech.edu; Warren.A.Holmes@jpl.nasa.gov NR 7 TC 5 Z9 5 U1 3 U2 50 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2100104 DI 10.1109/TASC.2012.2229375 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 080ZM UT WOS:000314283800063 ER PT J AU Brown, AD Chervenak, JA Chuss, D Mikula, V Ray, C Rostem, K U-yen, K Wassell, E Wollack, EJ AF Brown, Ari-David Chervenak, James A. Chuss, David Mikula, Vilem Ray, Christopher Rostem, Karwan U-yen, Kongpop Wassell, Edward Wollack, Edward J. TI Fabrication of Compact Superconducting Lowpass Filters for Ultrasensitive Detectors SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Dielectric thin films; metallic thin films; micro-machining; microwave filters; superconducting filters AB Optimal performance of background limited thermal detectors requires adequate control over all relevant sources of incident electromagnetic radiation. In addition to the radiant power incident from the scene of interest, undesired or spurious power can potentially couple to the sensor via its bias and readout circuitry employed to operate the device. One means of limiting the contribution of this stray radiation is to filter or block leakage associated with electrical connections in the detector environment. Here we discuss a fabrication methodology for realizing compact planar filters embedded in the wall of the detector enclosure whose tailored response controls the propagation of light through the far infrared. This approach consists of fabricating an array of boxed-stripline transmission line blocking filters to control thermal radiation incident via this path. Topologically, each superconducting center conductor is encased by a silicon dioxide dielectric insulator and surrounded by a metallic shield to form a single mode transmission line structure. We report on achieved attenuation and return loss and find that it replicates simulated data to a high degree. C1 [Brown, Ari-David; Chervenak, James A.; Chuss, David; U-yen, Kongpop; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mikula, Vilem] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Ray, Christopher; Wassell, Edward] MEI Technol Inc, Seabrook, MD 20706 USA. [Rostem, Karwan] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. RP Brown, AD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ari.d.brown@nasa.gov; james.a.chervanak@nasa.gov; david.t.chuss@nasa.gov; vilem.mikula@volny.cz; christopher.ray-1@nasa.gov; karwan.rostem@nasa.gov; kongpop.u-yen-1@nasa.gov; edward.wassell@nasa.gov; edward.j.wollack@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA; Research Opportunities in Space and Earth Sciences award [NNH09ZDA001N-APRA] FX This work was supported by NASA with a Research Opportunities in Space and Earth Sciences award in response to NNH09ZDA001N-APRA. This work was also supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 17 TC 2 Z9 2 U1 0 U2 38 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 2300204 DI 10.1109/TASC.2012.2231135 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 080ZM UT WOS:000314283800073 ER PT J AU Kleinsasser, A Chui, T Bumble, B Ladizinsky, E AF Kleinsasser, Alan Chui, Talso Bumble, Bruce Ladizinsky, Eric TI Critical Current Density and Temperature Dependence of Nb-Al Oxide-Nb Junction Resistance and Implications for Room Temperature Characterization SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Josephson junctions; superconducting devices; superconducting integrated circuits; superconducting thin films AB Room temperature junction resistance measurements are commonly used for screening Josephson-based circuits because testing is much easier than at cryogenic temperatures and can even be carried out at the wafer level. The value of ambient testing depends on the existence of a strong correspondence between the measured resistance at room temperature and the resistance and critical current obtained at the ultimate operating temperature. We have systematically studied the temperature dependence of junction resistance in order to quantify the emergence, with increasing critical current density, of parasitic contributions from non-uniform currents flowing in the Nb films, which tend to limit the value of room temperature screening. We will describe our measurements and our approach to correcting for these parasitic effects. C1 [Kleinsasser, Alan; Chui, Talso; Bumble, Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ladizinsky, Eric] D Wave Syst Inc, San Jose, CA 95134 USA. RP Kleinsasser, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alan.kleinsasser@jpl.nasa.gov; talso.c.chui@jpl.nasa.gov; bruce.bumble@jpl.nasa.gov; eric@dwavesys.com FU D-Wave Systems, Inc.; National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, and was supported in part by D-Wave Systems, Inc., and by the National Aeronautics and Space Administration. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, D-Wave Systems, Inc., or the Jet Propulsion Laboratory, California Institute of Technology. NR 12 TC 1 Z9 1 U1 1 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 1100405 DI 10.1109/TASC.2012.2228731 PN 1 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 080ZM UT WOS:000314283800004 ER PT J AU Williams, RME Grotzinger, JP Dietrich, WE Gupta, S Sumner, DY Wiens, RC Mangold, N Malin, MC Edgett, KS Maurice, S Forni, O Gasnault, O Ollila, A Newsom, HE Dromart, G Palucis, MC Yingst, RA Anderson, RB Herkenhoff, KE Le Mouelic, S Goetz, W Madsen, MB Koefoed, A Jensen, JK Bridges, JC Schwenzer, SP Lewis, KW Stack, KM Rubin, D Kah, LC Bell, JF Farmer, JD Sullivan, R Van Beek, T Blaney, DL Pariser, O Deen, RG AF Williams, R. M. E. Grotzinger, J. P. Dietrich, W. E. Gupta, S. Sumner, D. Y. Wiens, R. C. Mangold, N. Malin, M. C. Edgett, K. S. Maurice, S. Forni, O. Gasnault, O. Ollila, A. Newsom, H. E. Dromart, G. Palucis, M. C. Yingst, R. A. Anderson, R. B. Herkenhoff, K. E. Le Mouelic, S. Goetz, W. Madsen, M. B. Koefoed, A. Jensen, J. K. Bridges, J. C. Schwenzer, S. P. Lewis, K. W. Stack, K. M. Rubin, D. Kah, L. C. Bell, J. F., III Farmer, J. D. Sullivan, R. Van Beek, T. Blaney, D. L. Pariser, O. Deen, R. G. CA MSL Sci Team TI Martian Fluvial Conglomerates at Gale Crater SO SCIENCE LA English DT Article ID CHEMCAM INSTRUMENT SUITE; MERIDIANI-PLANUM; EARLY MARS; ROVER; SEDIMENT; SYSTEM; WATER; UNIT AB Observations by the Mars Science Laboratory Mast Camera (Mastcam) in Gale crater reveal isolated outcrops of cemented pebbles (2 to 40 millimeters in diameter) and sand grains with textures typical of fluvial sedimentary conglomerates. Rounded pebbles in the conglomerates indicate substantial fluvial abrasion. ChemCam emission spectra at one outcrop show a predominantly feldspathic composition, consistent with minimal aqueous alteration of sediments. Sediment was mobilized in ancient water flows that likely exceeded the threshold conditions (depth 0.03 to 0,9 meter, average velocity 0.20 to 0.75 meter per second) required to transport the pebbles. Climate conditions at the time sediment was transported must have differed substantially from the cold, hyper-arid modern environment to permit aqueous flows across several kilometers, C1 [Williams, R. M. E.; Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Grotzinger, J. P.; Stack, K. M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Dietrich, W. E.; Palucis, M. C.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Gupta, S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Sumner, D. Y.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Mangold, N.; Le Mouelic, S.] CNRS, LPGN, UMR6112, F-44322 Nantes, France. [Mangold, N.; Le Mouelic, S.] Univ Nantes, F-44322 Nantes, France. [Malin, M. C.; Edgett, K. S.; Van Beek, T.] Malin Space Sci Syst, San Diego, CA 92121 USA. [Maurice, S.; Forni, O.; Gasnault, O.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France. [Ollila, A.; Newsom, H. E.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Dromart, G.] Univ Lyon, Lab Geol Lyon, F-69364 Lyon, France. [Anderson, R. B.; Herkenhoff, K. E.] US Geol Survey, Flagstaff, AZ 86001 USA. [Goetz, W.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Madsen, M. B.; Koefoed, A.; Jensen, J. K.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Bridges, J. C.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Schwenzer, S. P.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Lewis, K. W.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Rubin, D.] US Geol Survey, Santa Cruz, CA 95060 USA. [Kah, L. C.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Bell, J. F., III; Farmer, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Sullivan, R.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Blaney, D. L.; Pariser, O.; Deen, R. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Williams, RME (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA. EM williams@psi.edu RI szopa, cyril/C-6865-2015; Harri, Ari-Matti/C-7142-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; Blanco, Juan Jose/E-3627-2014; Ramos, Miguel/K-2230-2014; Gomez, Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; Hayes, Alexander/P-2024-2014; Gasnault, Olivier/F-4327-2010; Zorzano, Maria-Paz/C-5784-2015; Madsen, Morten/D-2082-2011; Gonzalez, Rafael/D-1748-2009; Lemmon, Mark/E-9983-2010; Balic-Zunic, Tonci/A-6362-2013 OI Schwenzer, Susanne Petra/0000-0002-9608-0759; szopa, cyril/0000-0002-0090-4056; Harri, Ari-Matti/0000-0001-8541-2802; Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997; Edgett, Kenneth/0000-0001-7197-5751; Muller, Jan-Peter/0000-0002-5077-3736; Forni, Olivier/0000-0001-6772-9689; Blanco, Juan Jose/0000-0002-8666-0696; Ramos, Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060; Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Hayes, Alexander/0000-0001-6397-2630; Gasnault, Olivier/0000-0002-6979-9012; Zorzano, Maria-Paz/0000-0002-4492-9650; Madsen, Morten/0000-0001-8909-5111; Lemmon, Mark/0000-0002-4504-5136; Balic-Zunic, Tonci/0000-0003-1687-1233 FU NASA under the Mars Program Office [1449884, 1273887]; Centre National d'Etudes Spatiales; UK Space Agency; Danish Council for Independent Research/Natural Sciences (FNU) [12-127126, 11-107019]; TICRA Foundation; Deutsche Forschungsgemeinschaft [GO 2288/1-1] FX We thank K. Tanaka and L. Kestay (USGS-Flagstaff) and four anonymous referees for constructive reviews of this manuscript. This research was carried out for the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA under the Mars Program Office, including JPL contracts 1449884 (R.M.E.W.) and 1273887 (Malin Space Science Systems). Work in France was carried out with funding from the Centre National d'Etudes Spatiales. Work in the UK was funded by the UK Space Agency. Work in Denmark was funded by the Danish Council for Independent Research/Natural Sciences (FNU grants 12-127126 and 11-107019) and the TICRA Foundation. Work in Germany was partly funded by Deutsche Forschungsgemeinschaft grant GO 2288/1-1. Data in this manuscript arc available from the NASA Planetary Data System. This is PSI contribution 603. NR 35 TC 118 Z9 120 U1 8 U2 114 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 MAY 31 PY 2013 VL 340 IS 6136 BP 1068 EP 1072 DI 10.1126/science.1237317 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 154HJ UT WOS:000319664500037 PM 23723230 ER PT J AU Zeitlin, C Hassler, DM Cucinotta, FA Ehresmann, B Wimmer-Schweingruber, RF Brinza, DE Kang, S Weigle, G Bottcher, S Bohm, E Burmeister, S Guo, J Kohler, J Martin, C Posner, A Rafkin, S Reitz, G AF Zeitlin, C. Hassler, D. M. Cucinotta, F. A. Ehresmann, B. Wimmer-Schweingruber, R. F. Brinza, D. E. Kang, S. Weigle, G. Boettcher, S. Boehm, E. Burmeister, S. Guo, J. Koehler, J. Martin, C. Posner, A. Rafkin, S. Reitz, G. TI Measurements of Energetic Particle Radiation in Transit to Mars on the Mars Science Laboratory SO SCIENCE LA English DT Article ID SPACE EXPLORATION; TRANSPORT; MISSIONS AB The Mars Science Laboratory spacecraft, containing the Curiosity rover, was launched to Mars on 26 November 2011, and for most of the 253-day, 560-minion-kilometer cruise to Mars, the Radiation Assessment Detector made detailed measurements of the energetic particle radiation environment inside the spacecraft. These data provide insights into the radiation hazards that would be associated with a human mission to Mars. We report measurements of the radiation dose, dose equivalent, and linear energy transfer spectra. The dose equivalent for even the shortest round-trip with current propulsion systems and comparable shielding is found to be 0.66 +/- 0.12 sievert. C1 [Zeitlin, C.; Hassler, D. M.; Ehresmann, B.; Rafkin, S.] SW Res Inst, Boulder, CO USA. [Cucinotta, F. A.; Guo, J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Wimmer-Schweingruber, R. F.; Boettcher, S.; Boehm, E.; Burmeister, S.; Koehler, J.; Martin, C.] Univ Kiel, Kiel, Germany. [Brinza, D. E.; Kang, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Weigle, G.] SW Res Inst, San Antonio, TX USA. [Posner, A.] NASA Headquarters, Washington, DC USA. [Reitz, G.] German Aerosp Ctr DLR, Cologne, Germany. RP Zeitlin, C (reprint author), SW Res Inst, Boulder, CO USA. EM zeitlin@boulder.swri.edu OI Posner, Arik/0000-0003-1572-8734 FU NASA (Human Exploration and Operations Mission Directorate) under Jet Propulsion Laboratory (JPL) [1273039]; German Aerospace Center (DLR); DLR's Space Administration [50QM0501, 50 QM1201]; NASA FX The RAD is supported by NASA (Human Exploration and Operations Mission Directorate) under Jet Propulsion Laboratory (JPL) subcontract 1273039 to the Southwest Research Institute and in Germany by the German Aerospace Center (DLR) and DLR's Space Administration, grant numbers 50QM0501 and 50 QM1201, to the Christian Albrechts University, Kid. Part of this research was carried out at JPL, California Institute of Technology, under a contact with NASA. We appreciate discussions with P. O'Neill and M. Kim at NASA's JSC and with S. Blattnig, F. Badavi, T. Slaba, and C. Mertens of NASA's Langley Research Center. We extend thanks to I. Simmonds, I. Grotzinger, I. Crisp, A. Vasvada, H. Mortensen, and the Operations Product Generation Subsystem team at NASA-JPL. We also thank M. Meyer, E. Stolper, G. Allen, C. Moore, and V. Friedensen at NASA headquarters and H. Witte at DLR in Germany for their support of the RAD over the years. The data used in this paper are archived in the NASA Planetary Data System's Planetary Plasma Interactions Node at the University of California, Los Angeles. The archival volume includes the full binary raw data files, detailed descriptions of the structures therein, and higher-level data products in human-readable form. The PPI node is hosted at http://ppi.pds.nasa.gov/. NR 31 TC 104 Z9 107 U1 4 U2 41 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 MAY 31 PY 2013 VL 340 IS 6136 BP 1080 EP 1084 DI 10.1126/science.1235989 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 154HJ UT WOS:000319664500040 PM 23723233 ER PT J AU Moretto, P Zlotea, C Dolci, F Amieiro, A Bobet, JL Borgschulte, A Chandra, D Enoki, H De Rango, P Fruchart, D Jepsen, J Latroche, M Jansa, IL Moser, D Sartori, S Wang, SM Zan, JA AF Moretto, P. Zlotea, C. Dolci, F. Amieiro, A. Bobet, J. -L. Borgschulte, A. Chandra, D. Enoki, H. De Rango, P. Fruchart, D. Jepsen, J. Latroche, M. Jansa, I. Llamas Moser, D. Sartori, S. Wang, S. M. Zan, J. A. TI A Round Robin Test exercise on hydrogen absorption/desorption properties of a magnesium hydride based material SO INTERNATIONAL JOURNAL OF HYDROGEN ENERGY LA English DT Article DE Round Robin Test; Magnesium hydride; Kinetics; Thermodynamics; Enthalpy ID NANOCRYSTALLINE MAGNESIUM; STORAGE PROPERTIES; SYSTEMS AB A Round Robin Test exercise on magnesium hydride (MgH2) was performed by 14 laboratories with the aim to compare experimental isothermal data such PCI curves, kinetics curves and formation enthalpies together with a basic statistical evaluation of the results. The full hydrogen capacity was found to vary in the range 5.1-6.4 wt.% at 280 degrees C (553 K) and in the range 5.3-6.6 wt.% at 320 degrees C (593 K) (value for 1 MPa hydrogen pressure). The relative standard deviations of 6.9% and 7.2%, respectively, were measured for absorption. The absorption plateau pressure of magnesium hydride varies between 0.08 and 0.14 MPa with an average of 0.10 MPa and a relative standard deviation of 17.3% at 280 degrees C (553 K). At 320 degrees C (593 K) the absorption plateau pressure results fall in the range 0.26-0.45 MPa, with a relative standard deviation of 17.6%. Kinetics curves were affected by much higher data dispersion than the PCI data. The enthalpy of absorption was -75.7 KJ/moleH(2), with a relative standard deviation of 4.4%. The results highlight the importance of well defined measuring and reporting protocols as a base for future standard procedures. Copyright (C) 2013, Hydrogen Energy Publications, LLC. Published by Elsevier Ltd. All rights reserved. C1 [Moretto, P.; Zlotea, C.; Dolci, F.] European Commiss, Joint Res Ctr, Inst Energy & Transport, NL-1755 ZG Petten, Netherlands. [Amieiro, A.] Johnson Matthey Technol Ctr, Reading RG4 9NH, Berks, England. [Bobet, J. -L.] Univ Bordeaux 1, CNRS, ICMCB, F-33608 Pessac, France. [Borgschulte, A.] EMPA Mat Sci & Technol, Dept Mobil Environm & Energy, Diu Hydrogen & Energy, CH-8600 Dubendorf, Switzerland. [Chandra, D.] Univ Nevada, Met & Mat Engn Dept MS 388, Reno, NV 89557 USA. [Enoki, H.] Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki 3058565, Japan. [De Rango, P.; Fruchart, D.] CNRS, Inst NEEL, F-38042 Grenoble, France. [De Rango, P.; Fruchart, D.] CNRS, GRETA, F-38042 Grenoble, France. [Jepsen, J.] Helmholtz Zentrum Geesthacht, Dept Nanotechnol, D-21502 Geesthacht, Germany. [Latroche, M.] CNRS, ICMPE, UMR7182, F-94320 Thiais, France. [Jansa, I. Llamas] IFW Dresden, Inst Metall Werkstoffe, D-01171 Dresden, Germany. [Moser, D.] Univ Salford, Mat & Phys Res Ctr, Salford M5 4WT, Lancs, England. [Sartori, S.] Inst Energy Technol, NO-2027 Kjeller, Norway. [Wang, S. M.] GRINM Gen Res Inst Nonferrous Met, Beijing 100088, Peoples R China. [Zan, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Moretto, P (reprint author), European Commiss, Joint Res Ctr, Inst Energy & Transport, POB 2, NL-1755 ZG Petten, Netherlands. EM pietro.moretto@jrc.nl RI Moser, David/F-4590-2010; LATROCHE, MICHEL/L-6254-2014; Borgschulte, Andreas/D-5168-2016; Zlotea, Claudia/F-2954-2015 OI Moser, David/0000-0002-4895-8862; LATROCHE, MICHEL/0000-0002-8677-8280; Borgschulte, Andreas/0000-0001-6250-4667; FU European Commission DG Research [SES6-2006-518271/NESSHY] FX This work was conducted under the auspices of NESSHY European project. Funding by the European Commission DG Research (contract SES6-2006-518271/NESSHY) is gratefully acknowledged. The authors are very grateful to D. Baxter (JRC) who thoroughly reviewed the manuscript. NR 24 TC 10 Z9 10 U1 0 U2 32 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0360-3199 J9 INT J HYDROGEN ENERG JI Int. J. Hydrog. Energy PD MAY 30 PY 2013 VL 38 IS 16 BP 6704 EP 6717 DI 10.1016/j.ijhydene.2013.03.118 PG 14 WC Chemistry, Physical; Electrochemistry; Energy & Fuels SC Chemistry; Electrochemistry; Energy & Fuels GA 158GV UT WOS:000319958400017 ER PT J AU Temkin, A Shertzer, J AF Temkin, A. Shertzer, J. TI Electron scattering from excited states of hydrogen: Implications for the ionization threshold law SO PHYSICAL REVIEW A LA English DT Article ID ATOM IMPACT-IONIZATION; TEMKIN-POET MODEL AB The elastic scattering wave function for electrons scattered from the Nth excited state of hydrogen is the final state of the matrix element for excitation of that state. This paper deals with the solution of that problem primarily in the context of the Temkin-Poet (TP) model [A. Temkin, Phys. Rev. 126, 130 (1962); R. Poet, J. Phys. B 11, 3081 (1978)], wherein only the radial parts of the interaction are included. The relevant potential for the outer electron is dominated by the Hartree potential, V-N(H)(r). In the first part of the paper, V-N(H)(r) is approximated by a potential W-N(r), for which the scattering equation can be analytically solved. The results allow formal analytical continuation of N into the continuum, so that the ionization threshold law can be deduced. Because the analytic continuation involves going fromN to an imaginary function of the momentum of the inner electron, the threshold law turns out to be an exponentially damped function of the available energy E, in qualitative accord with the result of Macek and Ihra [J. H. Macek and W. Ihra, Phys. Rev. A 55, 2024 (1997)] for the TP model. Thereafter, the scattering equation for the Hartree potential V-N(H)(r) is solved numerically. The numerical aspects of these calculations have proven to be challenging and required several developments for the difficulties to be overcome. The results for V-N(H)(r) show only a simple energy-dependent shift from the approximate potential W-N(r), which therefore does not change the analytic continuation and the form of the threshold law. It is concluded that the relevant optical potential must be included in order to compare directly with the analytic result of Macek and Ihra. The paper concludes with discussions of (a) a quantum mechanical interpretation of the result, and (b) the outlook of this approach for the complete problem. C1 [Temkin, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shertzer, J.] Coll Holy Cross, Worcester, MA 01610 USA. [Shertzer, J.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Temkin, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 25 TC 0 Z9 0 U1 1 U2 5 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 MAY 30 PY 2013 VL 87 IS 5 AR 052718 DI 10.1103/PhysRevA.87.052718 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 155EF UT WOS:000319728500004 ER PT J AU Archibald, RF Kaspi, VM Ng, CY Gourgouliatos, KN Tsang, D Scholz, P Beardmore, AP Gehrels, N Kennea, JA AF Archibald, R. F. Kaspi, V. M. Ng, C. -Y. Gourgouliatos, K. N. Tsang, D. Scholz, P. Beardmore, A. P. Gehrels, N. Kennea, J. A. TI An anti-glitch in a magnetar SO NATURE LA English DT Article ID X-RAY PULSAR; VARIABLE SPIN-DOWN; NEUTRON-STARS; 1E 2259+586; SGR 1900+14; ROTATION; MAGNETOSPHERES; SUPERFLUIDITY; BURSTS AB Magnetars are neutron stars with X-ray and soft gamma-ray outbursts thought to be powered by intense internal magnetic fields(1). Like conventional neutron stars in the form of radio pulsars, magnetars exhibit 'glitches' during which angular momentum is believed to be transferred between the solid outer crust and the superfluid component of the inner crust(2-4). The several hundred observed glitches in radio pulsars(5,6) and magnetars(7) have involved a sudden spin-up (increase in the angular velocity) of the star, presumably because the interior superfluid was rotating faster than the crust. Here we report X-ray timing observations of the magnetar 1E 2259+586 (ref. 8), which exhibited a clear 'anti-glitch'-a sudden spin-down. We show that this event, like some previous magnetar spin-up glitches(9), was accompanied by multiple X-ray radiative changes and a significant spin-down rate change. Such behaviour is not predicted by models of neutron star spin-down and, if of internal origin, is suggestive of differential rotation in the magnetar, supporting the need for a rethinking of glitch theory for all neutron stars(10,11). C1 [Archibald, R. F.; Kaspi, V. M.; Ng, C. -Y.; Gourgouliatos, K. N.; Tsang, D.; Scholz, P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Ng, C. -Y.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Gehrels, N.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RP Kaspi, VM (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM vkaspi@physics.mcgill.ca RI Ng, Chi Yung/A-7639-2013; OI Ng, Chi Yung/0000-0002-5847-2612; Tsang, David/0000-0002-1612-2585; Gourgouliatos, Konstantinos N./0000-0002-1659-1250 FU Natural Sciences and Engineering Research Council of Canada; Canadian Institute for Advanced Research; Fonds de Recherche Nature et Technologies Quebec; Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology; Centre de Recherche en Astrophysique du Quebec FX V.M.K. acknowledges support from the Natural Sciences and Engineering Research Council of Canada Discovery Grant and the John C. Polanyi Award, from the Canadian Institute for Advanced Research, from Fonds de Recherche Nature et Technologies Quebec, from the Canada Research Chairs Program, and from the Lorne Trottier Chair in Astrophysics and Cosmology. D.T. was supported by the Lorne Trottier Chair in Astrophysics and Cosmology and the Canadian Institute for Advanced Research. K.N.G. was supported by the Centre de Recherche en Astrophysique du Quebec. We thank H. Medlin and J. Gelfand for help with the EVLA observation. We thank D. Eichler, B. Link, M. Lyutikov and C. Thompson for useful discussions. We acknowledge the use of public data from the Swift data archive. NR 26 TC 51 Z9 54 U1 0 U2 15 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 30 PY 2013 VL 497 IS 7451 BP 591 EP 593 DI 10.1038/nature12159 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 152UF UT WOS:000319556100037 PM 23719460 ER PT J AU Kleinbohl, A Wilson, RJ Kass, D Schofield, JT McCleese, DJ AF Kleinboehl, Armin Wilson, R. John Kass, David Schofield, John T. McCleese, Daniel J. TI The semidiurnal tide in the middle atmosphere of Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mars atmosphere; tides; semi-diurnal tide; MCS; water ice clouds; radiative effect ID GENERAL-CIRCULATION MODEL; DUSTY MARTIAN ATMOSPHERE; WATER ICE CLOUDS; THERMAL TIDES; DIURNAL TIDE; MGS TES; WAVES; VARIABILITY; ACCELEROMETER; TEMPERATURES AB Atmospheric thermal tides are global oscillations in atmospheric fields that are subharmonics of a solar day. While atmospheric tides on Earth are mainly relevant in the upper atmosphere, on Mars, they dominate temperature variations and winds throughout the atmosphere. Observations and model simulations to date have suggested that the migrating diurnal tide is the predominant mode in the Martian atmosphere, and that the semidiurnal tide is only relevant in the tropical middle atmosphere during conditions of high dust loading. New comprehensive observations by the Mars Climate Sounder in a geometry that allows coverage of multiple local times show that the semidiurnal tide is a dominant response of the Martian atmosphere throughout the Martian year. The maximum semidiurnal amplitude of similar to 16 K is found at southern winter high latitudes, which makes it the largest tidal amplitude observed in the Martian middle atmosphere outside of dust storm conditions. The semidiurnal tide can be successfully modeled due to recent advances of Mars General Circulation Models (MGCMs) that include the radiatively active treatment of water ice clouds. Tidal forcing occurs through absorption of radiation by aerosols and points to the vertical structure of dust and clouds and their radiative effects as being essential for our understanding of the thermal structure and the general circulation of the Martian atmosphere. As with terrestrial GCMs trying to quantify mechanisms affecting climate, future Mars modeling efforts will require microphysical schemes to control aerosol distributions, and vertically and temporally resolved measurements of temperature and aerosols will be essential for their validation. C1 [Kleinboehl, Armin; Kass, David; Schofield, John T.; McCleese, Daniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wilson, R. John] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. RP Kleinbohl, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Armin.Kleinboehl@jpl.nasa.gov FU NASA Planetary Atmospheres Program; National Aeronautics and Space Administration FX We are grateful to the MRO spacecraft team for keeping the MRO spacecraft alive and healthy and to the MCS instrument operations team for implementing and executing the MCS cross-track measurements. The contribution of R. J. W. was funded by the NASA Planetary Atmospheres Program. Work at the Jet Propulsion Laboratory, California Institute of Technology was performed under a contract with the National Aeronautics and Space Administration. The Editor thanks Jim Murphy and an anonymous reviewer for their assistance in evaluating this paper. NR 48 TC 14 Z9 14 U1 2 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 MAY 28 PY 2013 VL 40 IS 10 BP 1952 EP 1959 DI 10.1002/grl.50497 PG 8 WC Geosciences, Multidisciplinary SC Geology GA 277SS UT WOS:000328840200012 ER PT J AU Tian, YD Huffman, GJ Adler, RF Tang, L Sapiano, M Maggioni, V Wu, H AF Tian, Yudong Huffman, George J. Adler, Robert F. Tang, Ling Sapiano, Mathew Maggioni, Viviana Wu, Huan TI Modeling errors in daily precipitation measurements: Additive or multiplicative? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE uncertainty; precipitation; remote sensing; error modeling ID RAINFALL AB The definition and quantification of uncertainty depend on the error model used. For uncertainties in precipitation measurements, two types of error models have been widely adopted: the additive error model and the multiplicative error model. This leads to incompatible specifications of uncertainties and impedes intercomparison and application. In this letter, we assess the suitability of both models for satellite-based daily precipitation measurements in an effort to clarify the uncertainty representation. Three criteria were employed to evaluate the applicability of either model: (1) better separation of the systematic and random errors; (2) applicability to the large range of variability in daily precipitation; and (3) better predictive skills. It is found that the multiplicative error model is a much better choice under all three criteria. It extracted the systematic errors more cleanly, was more consistent with the large variability of precipitation measurements, and produced superior predictions of the error characteristics. The additive error model had several weaknesses, such as nonconstant variance resulting from systematic errors leaking into random errors, and the lack of prediction capability. Therefore, the multiplicative error model is a better choice. C1 [Tian, Yudong; Adler, Robert F.; Tang, Ling; Sapiano, Mathew; Maggioni, Viviana; Wu, Huan] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Tian, Yudong; Tang, Ling] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Huffman, George J.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. RP Tian, YD (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 617, Greenbelt, MD 20771 USA. EM Yudong.Tian@nasa.gov RI Huffman, George/F-4494-2014; Wu, Huan/K-1003-2013; Measurement, Global/C-4698-2015 OI Huffman, George/0000-0003-3858-8308; Wu, Huan/0000-0003-2920-8860; FU NASA Earth System Data Records Uncertainty Analysis Program [NNH10ZDA001N-ESDRERR] FX This research was supported by the NASA Earth System Data Records Uncertainty Analysis Program (Martha E. Maiden) under solicitation NNH10ZDA001N-ESDRERR. Computing resources were provided by the NASA Center for Climate Simulation. NR 27 TC 28 Z9 28 U1 2 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2013 VL 40 IS 10 BP 2060 EP 2065 DI 10.1002/grl.50320 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 277SS UT WOS:000328840200031 ER PT J AU Hall, DK Comiso, JC DiGirolamo, NE Shuman, CA Box, JE Koenig, LS AF Hall, Dorothy K. Comiso, Josefino C. DiGirolamo, Nicolo E. Shuman, Christopher A. Box, Jason E. Koenig, Lora S. TI Variability in the surface temperature and melt extent of the Greenland ice sheet from MODIS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Greenland melt; Greenland surface temperature; MODIS ID MASS-LOSS; PART II; SATELLITE; VALIDATION; SUMMIT; CLOUD AB Satellite-derived moderate-resolution imaging spectroradiometer (MODIS) ice-surface temperature (IST) of the Greenland ice sheet shows a positive trend and two major melt events from 2000 to present. IST increased by 0.550.44 degrees C/decade, with the greatest increase (0.950.44 degrees C/decade) found in northwestern Greenland where coastal temperatures and mass loss are also increasing and outlet glaciers are accelerating. IST shows the highest rates of increase during summer (1.350.47 degrees C/decade) and winter (1.301.53 degrees C/decade), followed by spring (0.60 +/- 0.98 degrees C/decade). In contrast, a decrease in IST was found in the autumn (-1.49 +/- 1.20 degrees C/decade). The IST trends in this work are not statistically significant with the exception of the trend in northwestern Greenland. Major surface melt (covering 80% or more of the ice sheet) occurred during the 2002 and 2012 melt seasons where clear-sky measurements show a maximum melt of 87% and 95% of the ice sheet surface, respectively. In 2002, most of the extraordinary melt was ephemeral, whereas in 2012 the ice sheet not only experienced more total melt, but melt was more persistent, and the 2012 summer was the warmest in the MODIS record (-6.38 +/- 3.98 degrees C). Our data show that major melt events may not be particularly rare during the present period of ice sheet warming. C1 [Hall, Dorothy K.; Comiso, Josefino C.; DiGirolamo, Nicolo E.; Shuman, Christopher A.; Koenig, Lora S.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [DiGirolamo, Nicolo E.] SSAI, Lanham, MD USA. [Shuman, Christopher A.] UMBC JCET, Baltimore, MD USA. [Box, Jason E.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. RP Hall, DK (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM Dorothy.k.hall@nasa.gov RI Box, Jason/H-5770-2013 NR 37 TC 43 Z9 45 U1 0 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2013 VL 40 IS 10 BP 2114 EP 2120 DI 10.1002/grl.50240 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 277SS UT WOS:000328840200041 ER PT J AU Hobbs, WR Willis, JK AF Hobbs, William R. Willis, Joshua K. TI Detection of an observed 135 year ocean temperature change from limited data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Ocean observation; Climate change; Detection and Attribution; Sea level rise ID PART I AB Recent work comparing historical hydrographic data with modern Argo observations shows a long-term change in the global ocean temperature. The magnitude of this change is greater than estimates of late 20(th) century warming, and implies a century-scale change in the global oceans. Using global coupled climate models from the Coupled Model Intercomparison Project Phase 5 suite of simulations, we assess to what extent this observed temperature difference can be attributed to a genuine long-term warming trend. After accounting for natural variability and sampling errors, we find convincing evidence that there has indeed been a century-scale anthropogenic warming of the global ocean up to the present day, and a strong possibility of anthropogenic warming from 1873 to 1955. The estimated 1873-1955 ocean warming implies a net top-of-atmosphere energy imbalance of 0.10.06 Wm(-2), and a thermosteric global mean sea level rise of 0.500.2 mma(-1). C1 [Hobbs, William R.] Univ Tasmania, Inst Marine & Antarctic Sci, Hobart, Tas 7001, Australia. [Willis, Joshua K.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hobbs, WR (reprint author), Univ Tasmania, Inst Marine & Antarctic Sci, Private Bag 129, Hobart, Tas 7001, Australia. EM whobbs@utas.edu.au RI Hobbs, Will/G-5116-2014 OI Hobbs, Will/0000-0002-2061-0899 FU National Aeronautics and Space Administration; Australian Research Council Centre of Excellence for Climate System Science [CE110001028] FX The authors wish to thank two anonymous reviewers for their helpful suggestions on improving this manuscript. This work was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration, and supported in part by the Australian Research Council Centre of Excellence for Climate System Science (grant CE110001028). NR 21 TC 4 Z9 4 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2013 VL 40 IS 10 BP 2252 EP 2258 DI 10.1002/grl.50370 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 277SS UT WOS:000328840200065 ER PT J AU Hall, TM Sobel, AH AF Hall, Timothy M. Sobel, Adam H. TI On the impact angle of Hurricane Sandy's New Jersey landfall SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE hurricanes; landfall risk ID CLIMATE-CHANGE; SURGE AB Hurricane Sandy's track crossed the New Jersey coastline at an angle closer to perpendicular than any previous hurricane in the historic record, one of the factors contributing to record-setting peak-water levels in parts of New Jersey and New York. To estimate the occurrence rate of Sandy-like tracks, we use a stochastic model built on historical hurricane data from the entire North Atlantic to generate a large sample of synthetic hurricanes. From this synthetic set we calculate that under long-term average climate conditions, a hurricane of Sandy's intensity or greater (category 1+) makes NJ landfall at an angle at least as close to perpendicular as Sandy's at an average annual rate of 0.0014 yr(-1) (95% confidence range 0.0007 to 0.0023); i.e., a return period of 714 years (95% confidence range 435 to 1429). C1 [Hall, Timothy M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Sobel, Adam H.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Sobel, Adam H.] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA. RP Hall, TM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM Timothy.M.Hall@nasa.gov RI Sobel, Adam/K-4014-2015 OI Sobel, Adam/0000-0003-3602-0567 FU NOAA [NA11OAR4310093]; NSF [AGS 1143959] FX We thank Kerry Emanuel for comments on the manuscript, as well as reviewer Chris Fogarty and an anonymous reviewer. This work was supported in part by NOAA grant NA11OAR4310093 and NSF grant AGS 1143959. NR 14 TC 30 Z9 30 U1 2 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2013 VL 40 IS 10 BP 2312 EP 2315 DI 10.1002/grl.50395 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 277SS UT WOS:000328840200076 ER PT J AU Schwartz, MJ Read, WG Santee, ML Livesey, NJ Froidevaux, L Lambert, A Manney, GL AF Schwartz, Michael J. Read, William G. Santee, Michelle L. Livesey, Nathaniel J. Froidevaux, Lucien Lambert, Alyn Manney, Gloria L. TI Convectively injected water vapor in the North American summer lowermost stratosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Anderson et al. (2012) (A2012) report in situobservations of convectively injected water vapor (H2O) in the North American (NA) summer lowermost stratosphere (LMS), occasionally exceeding 12ppmv. They contend that, in such cold/wet conditions, heterogeneous chemistry on binary watersulfate aerosols can activate chlorine, leading to catalytic ozone destruction. Aura Microwave Limb Sounder 100 hPa and 82.5 hPa H2O measurements show that, indeed, the NA LMS is unusually wet, both in mean values and in outliers reaching 18ppmv. Using A2012's threshold, 4% (0.03%) of 100 hPa (82.5 hPa) NA July-August observations are cold/wet enough for activation. Cold parcels, whether wet or dry, typically have much less HCl to activate and O(3)to destroy than A2012's initial conditions. Slightly lower concentrations of HCl and O-3 in cold/wet parcels are attributable, at least in part, to dilution by tropospheric air. Alarming reductions in NA summer column O(3)suggested by A2012 are not seen in the current climate. C1 [Schwartz, Michael J.; Read, William G.; Santee, Michelle L.; Livesey, Nathaniel J.; Froidevaux, Lucien; Lambert, Alyn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Manney, Gloria L.] NorthWest Res Associates, Socorro, NM USA. [Manney, Gloria L.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. RP Schwartz, MJ (reprint author), CALTECH, Jet Prop Lab, M-S 183-701, Pasadena, CA 91109 USA. EM michael.j.schwartz@jpl.nasa.gov RI Schwartz, Michael/F-5172-2016 OI Schwartz, Michael/0000-0001-6169-5094 NR 10 TC 13 Z9 13 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2013 VL 40 IS 10 BP 2316 EP 2321 DI 10.1002/grl.50421 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 277SS UT WOS:000328840200077 ER PT J AU von Clarmann, T Funke, B Lopez-Puertas, M Kellmann, S Linden, A Stiller, GP Jackman, CH Harvey, VL AF von Clarmann, T. Funke, B. Lopez-Puertas, M. Kellmann, S. Linden, A. Stiller, G. P. Jackman, C. H. Harvey, V. L. TI The solar proton events in 2012 as observed by MIPAS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE MIPAS; Solar proton event; stratosphere; mesosphere ID ATMOSPHERIC SOUNDING MIPAS; MICHELSON INTERFEROMETER; MESOSPHERE; RETRIEVAL; ENVISAT; N2O; ENHANCEMENTS; TEMPERATURE; NORTHERN; CLONO2 AB During the solar proton events (SPE) on 23-30 January and 7-15 March 2012, the Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) on Envisat monitored atmospheric temperature and composition with global coverage. In the Northern Hemisphere, the January SPE started at the end of a polar stratospheric warming period. The SPE effect is superimposed by large-scale subsidence of mesospheric NOx-rich air, which partly masks direct chemical SPE effects. SPE-induced NOx increases by 5, 20, 50, and 100 ppbv at altitudes of 50, 57, 60, and 70 km, respectively, are observed during the January SPE and those by 2, 5, 10, 20, 30, and 35 ppbv at altitudes of 47, 50, 53, 60, 63, and 66 km, respectively, during the March SPE. SPE-related ozone loss is clearly observed in the mesosphere, particularly in the tertiary ozone maximum. A sudden short-term HNO4 increase immediately after the January SPE hints at SPE-triggered HOx chemistry. In the Southern Hemisphere, a large NOx response is observed (increases by 2, 5, 10, 20, and 30 ppbv at 52, 56, 59, 63, and 70 km in January and by 2, 5, 10, 20, 30, and 35 ppbv at 47, 50, 53, 60, 63, and 66 km in March), while the effect on other species seems much less pronounced than in the Northern Hemisphere. SPE-related destruction of mesospheric ozone in the Southern Hemisphere was much more pronounced after the March SPE than the January SPE but in both cases, ozone recovered within about a day. C1 [von Clarmann, T.; Kellmann, S.; Linden, A.; Stiller, G. P.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany. [Funke, B.; Lopez-Puertas, M.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Jackman, C. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Harvey, V. L.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP von Clarmann, T (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res, POB 3640, D-76021 Karlsruhe, Germany. EM Thomas.Clarmann@Kit.Edu RI Jackman, Charles/D-4699-2012; Funke, Bernd/C-2162-2008; Lopez Puertas, Manuel/M-8219-2013; Stiller, Gabriele/A-7340-2013 OI Funke, Bernd/0000-0003-0462-4702; Lopez Puertas, Manuel/0000-0003-2941-7734; Stiller, Gabriele/0000-0003-2883-6873 FU Spanish MCINN [AYA2011-23552]; EC FEDER funds; Deutsche Forschungsgemeinschaft; Karlsruhe Institute of Technology FX ESA has provided MIPAS level-1B data. The IAA team was supported by the Spanish MCINN under grant AYA2011-23552 and EC FEDER funds. We acknowledge support by Deutsche Forschungsgemeinschaft and Open Access Publishing Fund of Karlsruhe Institute of Technology. NR 23 TC 17 Z9 17 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2013 VL 40 IS 10 BP 2339 EP 2343 DI 10.1002/grl.50119 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 277SS UT WOS:000328840200081 ER PT J AU Shi, Y Yoonessi, M Weiss, RA AF Shi, Ying Yoonessi, Mitra Weiss, R. A. TI High Temperature Shape Memory Polymers SO MACROMOLECULES LA English DT Article ID ETHER KETONE) MEMBRANES; METHANOL FUEL-CELLS; SULFURIC-ACID; IONOMERS; PEEK; SULFONATION; COMPOSITES; MECHANISM; KINETICS; NETWORK AB High switching temperature shape memory polymers (SMPs) were developed from metal salts of sulfonated PEEK (M-SPEEK) ionomer and composites of the M-SPEEK ionomers and a fatty acid salt. The neat M-SPEEK ionomers exhibited reasonable shape memory behavior, but the composite SMPs showed very promising shape memory behavior. The composites were prepared from 70 wt % M-SPEEK (M = sodium or zinc) and 30 wt % sodium oleate (NaOl). Ionic nanodomains formed by the interactions of ionic groups provided a permanent physically cross-linked network, and strong dipolar interactions between the ionomer and a dispersed phase of crystalline NaOl provided the temporary network. A temporary shape was achieved and fixed by deforming the material above the melting temperature (T-m) of NaOl and then cooling under stress to below T-m. The permanent shape was recovered by reheating the material above T-m without applying stress. Shape fixing efficiencies of 96% were achieved, and shape recovery reached 100%. Triple shape memory behavior was also achieved for M-SPEEK/NaOl compounds using the glass transition of the ionomer and the melting point of the NaOl as two separate switching temperatures. C1 [Shi, Ying; Weiss, R. A.] Univ Akron, Dept Polymer Engn, Akron, OH 44325 USA. [Yoonessi, Mitra] NASA, Ohio Aerosp Inst, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Weiss, RA (reprint author), Univ Akron, Dept Polymer Engn, Akron, OH 44325 USA. EM rweiss@uakron.edu FU Ohio Space Grant Consortium (OSGC)/NASA; Polymer Division of the National Science Foundation [DMR-0960461] FX This research was partially supported by Ohio Space Grant Consortium (OSGC)/NASA and partially supported by a grant from the Polymer Division of the National Science Foundation (DMR-0960461). NR 39 TC 37 Z9 37 U1 6 U2 74 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0024-9297 J9 MACROMOLECULES JI Macromolecules PD MAY 28 PY 2013 VL 46 IS 10 BP 4160 EP 4167 DI 10.1021/ma302670p PG 8 WC Polymer Science SC Polymer Science GA 156BQ UT WOS:000319795800050 ER PT J AU Vallisneri, M Yunes, N AF Vallisneri, Michele Yunes, Nicolas TI Stealth bias in gravitational-wave parameter estimation SO PHYSICAL REVIEW D LA English DT Article ID INSPIRALLING COMPACT BINARIES; BLACK-HOLE COALESCENCES; GRAVITY; MERGER; LISA AB Inspiraling binaries of compact objects are primary targets for current and future gravitational-wave observatories. Waveforms computed in general relativity are used to search for these sources, and will probably be used to extract source parameters from detected signals. However, if a different theory of gravity happens to be correct in the strong-field regime, source-parameter estimation may be affected by a fundamental bias: that is, by systematic errors due to the use of waveforms derived in the incorrect theory. If the deviations from general relativity are not large enough to be detectable on their own and yet these systematic errors remain significant (i.e., larger than the statistical uncertainties in parameter estimation), fundamental bias cannot be corrected in a single observation, and becomes stealth bias. In this article we develop a scheme to determine in which cases stealth bias could be present in gravitational-wave astronomy. For a given observation, the answer depends on the detection signal-to-noise ratio and on the strength of the modified-gravity correction. As an example, we study three representative stellar-mass binary systems that will be detectable with second-generation ground-based observatories. We find that significant systematic bias can occur whether or not modified gravity can be positively detected, for correction strengths that are not currently excluded by any other experiment. Thus, stealth bias may be a generic feature of gravitational-wave detections, and it should be considered and characterized, using expanded models such as the parametrized post-Einstein framework, when interpreting the results of parameter-estimation analyses. C1 [Vallisneri, Michele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yunes, Nicolas] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Vallisneri, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. FU NSF Grant [PHY-1114374]; NASA Grant [NNX11AI49G, 00001944, NNX10AC69G]; National Space and Aeronautics Administration FX We thank Curt Cutler for useful comments and suggestions, Katerina Chatziioannou for providing details about the Picard-Lindelof and Cauchy-Lipschitz uniqueness theorems, Neil Cornish and Laura Sampson for help in validating our Fisher calculations with Cornish's MCMC code in certain simplified cases, and the organizers of the 2011 Astro-GR workshop, where this work was conceived. N. Y. acknowledges support from NSF Grant No. PHY-1114374 and NASA Grant No. NNX11AI49G, under Subaward No. 00001944. M.V.'s research was supported by NASA Grant No. NNX10AC69G, and was performed at the Jet Propulsion Laboratory under contract with the National Space and Aeronautics Administration. NR 53 TC 14 Z9 14 U1 1 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD MAY 28 PY 2013 VL 87 IS 10 AR 102002 DI 10.1103/PhysRevD.87.102002 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 154FE UT WOS:000319656400001 ER PT J AU Eyring, V Arblaster, JM Cionni, I Sedlacek, J Perliwitz, J Young, PJ Bekki, S Bergmann, D Cameron-Smith, P Collins, WJ Faluvegi, G Gottschaldt, KD Horowitz, LW Kinnison, DE Lamarque, JF Marsh, DR Saint-Martin, D Shindell, DT Sudo, K Szopa, S Watanabe, S AF Eyring, V. Arblaster, J. M. Cionni, I. Sedlacek, J. Perliwitz, J. Young, P. J. Bekki, S. Bergmann, D. Cameron-Smith, P. Collins, W. J. Faluvegi, G. Gottschaldt, K. D. Horowitz, L. W. Kinnison, D. E. Lamarque, J. F. Marsh, D. R. Saint-Martin, D. Shindell, D. T. Sudo, K. Szopa, S. Watanabe, S. TI Long-term ozone changes and associated climate impacts in CMIP5 simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE CMIP5; stratospheric ozone; stratospheric temperature; zonal wind changes; troposheric ozone; chemistry-climate coupling ID GENERAL-CIRCULATION MODEL; STRATOSPHERIC TEMPERATURE TRENDS; EARTH SYSTEM MODEL; TROPOSPHERIC OZONE; ATMOSPHERIC CHEMISTRY; COUPLED MODEL; GISS MODELE; SEA-ICE; AEROSOLS; GAS AB Ozone changes and associated climate impacts in the Coupled Model Intercomparison Project Phase 5 (CMIP5) simulations are analyzed over the historical (1960-2005) and future (2006-2100) period under four Representative Concentration Pathways (RCP). In contrast to CMIP3, where half of the models prescribed constant stratospheric ozone, CMIP5 models all consider past ozone depletion and future ozone recovery. Multimodel mean climatologies and long-term changes in total and tropospheric column ozone calculated from CMIP5 models with either interactive or prescribed ozone are in reasonable agreement with observations. However, some large deviations from observations exist for individual models with interactive chemistry, and these models are excluded in the projections. Stratospheric ozone projections forced with a single halogen, but four greenhouse gas (GHG) scenarios show largest differences in the northern midlatitudes and in the Arctic in spring (approximate to 20 and 40 Dobson units (DU) by 2100, respectively). By 2050, these differences are much smaller and negligible over Antarctica in austral spring. Differences in future tropospheric column ozone are mainly caused by differences in methane concentrations and stratospheric input, leading to approximate to 10 DU increases compared to 2000 in RCP 8.5. Large variations in stratospheric ozone particularly in CMIP5 models with interactive chemistry drive correspondingly large variations in lower stratospheric temperature trends. The results also illustrate that future Southern Hemisphere summertime circulation changes are controlled by both the ozone recovery rate and the rate of GHG increases, emphasizing the importance of simulating and taking into account ozone forcings when examining future climate projections. C1 [Eyring, V.; Gottschaldt, K. D.] Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atomosphare, Oberpfaffenhofen, Germany. [Arblaster, J. M.] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia. [Arblaster, J. M.; Kinnison, D. E.; Lamarque, J. F.; Marsh, D. R.] Natl Ctr Atmospher Res, Boulder, CO USA. [Cionni, I.] Energia Sviluppo Econ Sostenibile, Agenzia Nazl Nuove Tecnol, Bologna, Italy. [Sedlacek, J.] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Perliwitz, J.; Young, P. J.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Perliwitz, J.; Young, P. J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO USA. [Bekki, S.; Szopa, S.] Inst Pierre Simon Laplace, Paris, France. [Bergmann, D.; Cameron-Smith, P.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Collins, W. J.] Met Off Hadely Ctr, Exeter, Devon, England. [Faluvegi, G.; Shindell, D. T.] NASA, Goddard Inst Space Studies, New York, NY USA. [Horowitz, L. W.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Saint-Martin, D.] CNRM GAME, Toulouse, France. [Sudo, K.] Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi, Japan. [Watanabe, S.] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan. RP Eyring, V (reprint author), Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atomosphare, Oberpfaffenhofen, Germany. EM veronika.eyring@dlr.de RI Eyring, Veronika/O-9999-2016; Watanabe, Shingo/L-9689-2014; Manager, CSD Publications/B-2789-2015; bekki, slimane/J-7221-2015; Arblaster, Julie/C-1342-2010; Perlwitz, Judith/B-7201-2008; Sedlacek, Jan/B-2819-2009; Szopa, Sophie/F-8984-2010; Collins, William/A-5895-2010; Shindell, Drew/D-4636-2012; Horowitz, Larry/D-8048-2014; Bergmann, Daniel/F-9801-2011; Young, Paul/E-8739-2010; Marsh, Daniel/A-8406-2008; Lamarque, Jean-Francois/L-2313-2014; Cameron-Smith, Philip/E-2468-2011 OI Eyring, Veronika/0000-0002-6887-4885; Watanabe, Shingo/0000-0002-2228-0088; Gottschaldt, Klaus/0000-0002-2046-6137; bekki, slimane/0000-0002-5538-0800; Arblaster, Julie/0000-0002-4287-2363; Perlwitz, Judith/0000-0003-4061-2442; Sedlacek, Jan/0000-0002-6742-9130; Szopa, Sophie/0000-0002-8641-1737; Collins, William/0000-0002-7419-0850; Horowitz, Larry/0000-0002-5886-3314; Bergmann, Daniel/0000-0003-4357-6301; Young, Paul/0000-0002-5608-8887; Marsh, Daniel/0000-0001-6699-494X; Lamarque, Jean-Francois/0000-0002-4225-5074; Cameron-Smith, Philip/0000-0002-8802-8627 NR 182 TC 79 Z9 80 U1 4 U2 59 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 5029 EP 5060 DI 10.1002/jgrd.50316 PG 32 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000081 ER PT J AU Burgener, L Rupper, S Koenig, L Forster, R Christensen, WF Williams, J Koutnik, M Miege, C Steig, EJ Tingey, D Keeler, D Riley, L AF Burgener, Landon Rupper, Summer Koenig, Lora Forster, Rick Christensen, William F. Williams, Jessica Koutnik, Michelle Miege, Clement Steig, Eric J. Tingey, David Keeler, Durban Riley, Laura TI An observed negative trend in West Antarctic accumulation rates from 1975 to 2010: Evidence from new observed and simulated records SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE West Antarctica; accumulation rate; Southern Annular Mode; SAM; firn core ID SOUTHERN ANNULAR MODE; INTERNATIONAL GEOPHYSICAL YEAR; SURFACE MASS-BALANCE; GLOBAL CLIMATE MODEL; ICE-SHEET; SEA-ICE; SNOW ACCUMULATION; VARIABILITY; PRECIPITATION; CIRCULATION AB Observations of snow accumulation rates from five new firn cores show a negative trend that is statistically significant over the past several decades across the central West Antarctic ice sheet (WAIS). A negative temporal trend in accumulation rates is unexpected in light of rising surface temperatures as well as model simulations predicting higher accumulation rates for the region. Both the magnitude of the mean accumulation rates and the range of interannual variability observed in the new records compare favorably to older records collected from a broad area of the WAIS, suggesting that the new data may serve as a regional proxy for recent temporal trends in West Antarctic accumulation rates. The observed negative trend in accumulation is likely the result of a shift in low-pressure systems over the Amundsen Sea region, dominated by changes in the austral fall season. Regional-scale climate models and reanalysis data do not capture the negative trend in accumulation rate observed in these firn cores. Nevertheless the models and reanalyses agree well in both accumulation-rate means and interannual variability, with no single model or dataset standing out as significantly more skilled at capturing the observed magnitude of and trend in accumulation rates in this region of the WAIS. C1 [Burgener, Landon; Rupper, Summer; Christensen, William F.; Williams, Jessica; Tingey, David; Keeler, Durban; Riley, Laura] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. [Koenig, Lora] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Forster, Rick; Miege, Clement] Univ Utah, Dept Geog, Salt Lake City, UT USA. [Koutnik, Michelle] Univ Copenhagen, Niels Bohr Inst, Ctr Ice & Climate, DK-2100 Copenhagen, Denmark. [Steig, Eric J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. RP Rupper, S (reprint author), Brigham Young Univ, Dept Geol Sci, S389 ESC, Provo, UT 84602 USA. EM srupper@byu.edu RI Steig, Eric/G-9088-2015; OI Steig, Eric/0000-0002-8191-5549; Rupper, Summer/0000-0001-8655-5282; Miege, Clement/0000-0002-1894-3723 FU National Science Foundation Office of Polar Programs [094470, 0944653]; NASA's Cryospheric Sciences Program FX This work was supported by the National Science Foundation Office of Polar Programs (grant 094470 to SBR and 0944653 to RF) and NASA's Cryospheric Sciences Program (to LSK). The authors thank David Battisti and Qinghua Ding for feedback on the methods and science. The authors also thank three anonymous reviewers for constructive comments and criticisms that significantly improved the manuscript. NR 53 TC 9 Z9 9 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4205 EP 4216 DI 10.1002/jgrd.50362 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000020 ER PT J AU Li, KF Tian, BJ Tung, KK Kuai, L Worden, JR Yung, YL Slawski, BL AF Li, King-Fai Tian, Baijun Tung, Ka-Kit Kuai, Le Worden, John R. Yung, Yuk L. Slawski, Benjiman L. TI A link between tropical intraseasonal variability and Arctic stratospheric ozone SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Madden-Julian Oscillation; teleconnection; geopotential heights; barotropic propagation; tropopause motions ID MADDEN-JULIAN OSCILLATION; TROPOSPHERIC EMISSION SPECTROMETER; MOIST THERMODYNAMIC STRUCTURE; NORTHERN-HEMISPHERE WINTER; MONITORING INSTRUMENT; INTERIM REANALYSIS; AURA SATELLITE; KELVIN WAVE; MJO; SYSTEM AB Previous studies using satellite measurements showed evidence that subtropical upper troposphere/lower stratosphere ozone (O-3) can be modulated by tropical intraseasonal variability, the most dominant form of which is the Madden Julian Oscillation (MJO) with a period of 30-60days. Here we further study the MJO modulation in the upper troposphere/lower stratosphere O-3 over the northern extratropics and the Arctic. Significant MJO-related O-3 signals (13-20 Dobson units) are found over the northern extratropics (north of 30 degrees N). The O-3 anomalies change their magnitude and patterns depending on the phase of the MJO. Over the Arctic, the MJO-related O-3 anomalies are dominated by a wave number 2 structure and are anticorrelated with the geopotential height (GPH) anomalies at 250hPa. The latter is similar to the findings in the previous studies over subtropics and indicates that the Arctic upper troposphere/lower stratosphere O-3 anomalies are associated with dynamical motions near the tropopause. The teleconnection from the tropics to the Arctic is likely through propagation of planetary waves generated by the equatorial heating that affects the tropopause height and O-3 at high latitudes. C1 [Li, King-Fai; Yung, Yuk L.; Slawski, Benjiman L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Tian, Baijun; Kuai, Le; Worden, John R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tung, Ka-Kit] Univ Washington, Dept Appl Math, Seattle, WA 98195 USA. RP Li, KF (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM kfl@gps.caltech.edu OI Tian, Baijun/0000-0001-9369-2373; Li, King-Fai/0000-0003-0150-2910 FU National Aeronautics and Space Administration (NASA) [JPL-1429248]; National Science Foundation (NSF) [ATM-0840755, ATM-0934303] FX K. F. L. is grateful to Prof. Simona Bordoni, Prof. Duane E. Waliser, and Dr. Xianan Jiang for their thoughtful comments. K. F. L. and Y.L.Y. were supported by National Aeronautics and Space Administration (NASA) grant JPL-1429248 to the California Institute of Technology. B.J. was supported by National Science Foundation (NSF) award ATM-0840755 to the University of California, Los Angeles. B. L. S. was supported by NSF grant ATM-0934303. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The RMM index was obtained from http://www.cawcr.gov.au/staff/mwheeler/maproom/RMM/RMM1RMM2.74toRealtime .txt. NR 71 TC 2 Z9 2 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4280 EP 4289 DI 10.1002/jgrd.50391 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000026 ER PT J AU Segal-Rosenheimer, M Russell, PB Livingston, JM Ramachandran, S Redemann, J Baum, BA AF Segal-Rosenheimer, Michal Russell, Philip B. Livingston, John M. Ramachandran, S. Redemann, Jens Baum, Bryan A. TI Retrieval of cirrus properties by Sun photometry: A new perspective on an old issue SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE cirrus microphysical properties; cirrus optical depth; Sun photometers; cloud optics; aerosols and clouds ID AEROSOL OPTICAL DEPTH; BULK SCATTERING PROPERTIES; SOLAR RADIATIVE-TRANSFER; PARTICLE-SIZE; ICE CLOUDS; THICKNESS; DISTRIBUTIONS; VARIABILITY; ALGORITHMS; ABSORPTION AB Cirrus clouds are important modulators of the Earth radiation budget and continue to be one of the most uncertain components in weather and climate modeling. Sun photometers are widely accepted as one of the most accurate platforms for measuring clear sky aerosol optical depth (AOD). However, interpretation of their measurements is ambiguous in the presence of cirrus. Derivation of a valid AOD under cirrus conditions was focused previously on correction factors, rather than on derivation of cirrus cloud optical thickness (COT). In the present work, we propose a new approach that uses the total measured irradiance to derive cirrus COT and ice particle effective diameter (D-eff). For this approach, we generate lookup tables (LUTs) of total transmittance for the Sun photometer field of view (FOV) due to the direct and scattered irradiance over the spectral range of 400-2200 nm, for a range of cirrus COT (0-4), and a range of ice cloud effective diameters (10-120 mu m) by using explicit cirrus optical property models for (a) cirrus only and (b) a two-component model including cirrus and aerosols. The new approach is tested on two cases (airborne and ground-based) using measured transmittances from the 14-channel NASA Ames Airborne Tracking Sun photometer. We find that relative uncertainties in COT are much smaller than those for D-eff. This study shows that for optically thin cirrus cases (COT<1.0), the aerosol layer between the instrument and the cloud plays an important role, especially in derivation of D-eff. Additionally, the choice of the cirrus model may introduce large differences in derived D-eff. C1 [Segal-Rosenheimer, Michal; Russell, Philip B.; Redemann, Jens] NASA Ames Res Ctr, Moffett Field, CA USA. [Livingston, John M.] SRI Int, Menlo Pk, CA 94025 USA. [Ramachandran, S.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Baum, Bryan A.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. RP Segal-Rosenheimer, M (reprint author), NASA Ames Res Ctr, Moffett Field, CA USA. EM michal.segalrozenhaimer@nasa.gov RI Baum, Bryan/B-7670-2011 OI Baum, Bryan/0000-0002-7193-2767 FU ORAU (Oak-Ridge Associated Universities) NPP (NASA Post-doctoral Program); Weizmann Institute through the Women in Science program; ORAU-NPP FX Michal Segal-Rosenheimer would like to thank the ORAU (Oak-Ridge Associated Universities) NPP (NASA Post-doctoral Program) and the Weizmann Institute through the Women in Science program for the financial support for her Post-doctoral fellowship at the NASA Ames Research Center. S Ramachandran would also like to thank ORAU-NPP for his support. The ARCTAS measurements were supported by the NASA Radiation and Science Program. We appreciate the comments of the three anonymous reviewers, which helped us to improve the manuscript. NR 37 TC 6 Z9 6 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4503 EP 4520 DI 10.1002/jgrd.50185 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000043 ER PT J AU Huang, L Jiang, JH Tackett, JL Su, H Fu, R AF Huang, Lei Jiang, Jonathan H. Tackett, Jason L. Su, Hui Fu, Rong TI Seasonal and diurnal variations of aerosol extinction profile and type distribution from CALIPSO 5-year observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE CALIPSO; aerosol extinction; aerosol type; aerosol seasonal variation; aerosol diurnal variation ID SATELLITE-OBSERVATIONS; UPPER TROPOSPHERE; CLOUDS; MODEL; SMOKE; LIDAR; TRANSPORT; PRECIPITATION; INHIBITION; ALGORITHM AB The new Level 3 aerosol profile data derived from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) provide a multiyear global aerosol distribution with high vertical resolution. We analyzed seasonal and diurnal variations of the vertical distributions of aerosol properties represented by 5-year CALIPSO data. Results show that dust, smoke, and polluted dust are the most frequently detected aerosol types during all seasons. Dust is the dominant type, especially in the middle to upper troposphere, over most areas during boreal spring and summer, while smoke and polluted dust tend to dominate during biomass burning seasons. The seasonal variations of dust layer top height and dust contribution to all-aerosol extinction are positively correlated with the seasonal variation of the dust occurrence frequency. The seasonal cycle of aerosol properties over west Australia is similar to that over biomass burning regime areas, despite its desert regime. In general, smoke is detected more frequently from the lower to middle troposphere; clean marine and polluted continental aerosols are detected more frequently, while polluted dust is detected less frequently, in the lower troposphere during nighttime than daytime. The all-aerosol extinction is generally larger, and the aerosol layer top is detected at high altitudes more frequently during nighttime than daytime. The diurnal changes of aerosol properties are similar within the same aerosol regime. Dust extinction shows little diurnal variation except when dust is the dominant aerosol type. The results contribute to an initial global 3-D aerosol climatology which will likely be extended and improved in the future. C1 [Huang, Lei; Fu, Rong] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX USA. [Jiang, Jonathan H.; Su, Hui] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Tackett, Jason L.] Sci Syst & Applicat Inc, Hampton, VA USA. RP Huang, L (reprint author), Univ Texas Austin, Dept Geol Sci, Univ Stn C1100, Austin, TX 78712 USA. EM leih@utexas.edu RI Huang, Lei/P-1848-2014 FU NASA Aura Science Team program [NNX11AE72G]; Jackson School of Geosciences at the University of Texas at Austin; JPL Graduate Fellowship Program; NASA FX This research was supported by the NASA Aura Science Team program (NNX11AE72G) and the Jackson School of Geosciences at the University of Texas at Austin. Most of this study was performed at NASA Jet Propulsion Laboratory (JPL) at the California Institute of Technology, under contract with NASA. The first author thanks support from the JPL Graduate Fellowship Program. The third author would like to thank Ali Omar and Stuart Young for input on CALIPSO aerosol typing. We also appreciate the comments from four anonymous reviewers that led to significant improvements of this paper. The CALIPSO Level 3 data were obtained from the Atmospheric Science Data Center at NASA Langley Research Center. NR 54 TC 11 Z9 12 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4572 EP 4596 DI 10.1002/jgrd.50407 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000047 ER PT J AU Toth, TD Zhang, JL Campbell, JR Reid, JS Shi, YX Johnson, RS Smirnov, A Vaughan, MA Winker, DM AF Toth, Travis D. Zhang, Jianglong Campbell, James R. Reid, Jeffrey S. Shi, Yingxi Johnson, Randall S. Smirnov, Alexander Vaughan, Mark A. Winker, David M. TI Investigating enhanced Aqua MODIS aerosol optical depth retrievals over the mid-to-high latitude Southern Oceans through intercomparison with co-located CALIOP, MAN, and AERONET data sets SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol; sea salt; MODIS; satellite; CALIPSO; MAN ID CLOUD CONTAMINATION; DATA-ASSIMILATION; SATELLITE DATA; GOCART MODEL; PART I; CALIPSO; ALGORITHM; PRODUCTS; VALIDATION; THICKNESS AB A band of enhanced aerosol optical depth (AOD) over the mid-to-high latitude Southern Oceans exists in some passive satellite-based aerosol data sets, including Moderate Resolution Imaging Spectroradiometer (MODIS) products. Past studies suggest several potential causes contributing to this phenomenon, including signal uncertainty, retrieval bias, and cloud contamination. In this paper, quality-assured Aqua MODIS aerosol products in this zonal band are investigated to assess cloud contamination as a cause. Spatially and temporally collocated cloud and aerosol products produced by the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) project relative to Aqua MODIS AOD in this region are considered. Maritime Aerosol Network (MAN) and Aerosol Robotic Network (AERONET) AOD data are also collocated with Aqua MODIS retrievals for surface context. The results of this study indicate that the high Aqua MODIS AOD are not seen in the CALIOP aerosol products, cannot be screened using active profiling of collocated observations for cloud presence, and are not detected by ground-based observations such as MAN and AERONET. Enhanced AOD values are attributable primarily to stratocumulus and low broken cumulus cloud contamination, as identified with CALIOP products. But these clouds explain only about 30-40% of the total anomaly. Cirrus cloud contamination is also a factor. However, in contrast to the rest of the globe, they contribute less overall, relative to low-level liquid water clouds, which are considered likely the result of misidentification of relatively warm cloud tops compared with surrounding open seas. C1 [Toth, Travis D.; Zhang, Jianglong; Shi, Yingxi; Johnson, Randall S.] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. [Campbell, James R.; Reid, Jeffrey S.] Naval Res Lab, Marine Meteorol Div, Aerosol & Radiat Sci Sect, Monterey, CA USA. [Smirnov, Alexander] Sigma Space Corp, Greenbelt, MD USA. [Vaughan, Mark A.; Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Zhang, JL (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA. EM jzhang@atmos.und.edu RI Reid, Jeffrey/B-7633-2014; Campbell, James/C-4884-2012 OI Reid, Jeffrey/0000-0002-5147-7955; Campbell, James/0000-0003-0251-4550 FU Office of Naval Research [32, 35]; NASA Interagency Agreement [NNG12HG05I]; NASA Earth and Space Science Fellowship (NESSF) Program FX This research was funded through the support of the Office of Naval Research Codes 32 and 35. Author JRC acknowledges the support of NASA Interagency Agreement NNG12HG05I on behalf of the NASA Micropulse Lidar Network. Author YS acknowledges the support of the NASA Earth and Space Science Fellowship (NESSF) Program. CALIPSO data were obtained from the NASA Langley Research Center Atmospheric Science Data Center. MODIS data were obtained from NASA Goddard Space Flight Center. We acknowledge the AERONET and MAN programs, their contributing principal investigators and their staff for coordinating the sites and data used for this investigation. NR 53 TC 17 Z9 18 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4700 EP 4714 DI 10.1002/jgrd.50311 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000056 ER PT J AU Omar, AH Winker, DM Tackett, JL Giles, DM Kar, J Liu, Z Vaughan, MA Powell, KA Trepte, CR AF Omar, A. H. Winker, D. M. Tackett, J. L. Giles, D. M. Kar, J. Liu, Z. Vaughan, M. A. Powell, K. A. Trepte, C. R. TI CALIOP and AERONET aerosol optical depth comparisons: One size fits none SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Aerosol Optical Depth; AERONET; CALIPSO ID CLOUD CONTAMINATION; MODIS-AQUA; VALIDATION; ALGORITHM; CALIPSO; RETRIEVAL; PROFILES; PRODUCTS; NETWORK; OCEAN AB We compare the aerosol optical depths (AOD) retrieved from backscatter measurements of the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) aboard the Cloud Aerosol Lidar Infrared Pathfinder Satellite Observations (CALIPSO) satellite with coincident Aerosol Robotic Network (AERONET) measurements. Overpass coincidence criteria of 2h and within a 40km radius are satisfied at least once at 149 globally distributed AERONET sites from 2006 to 2010. Most data pairs (>80%) use AERONET measurements acquired 30min of the overpass. We examine the differences in AOD estimates between CALIOP and AERONET for various aerosol, environmental, and geographic conditions. Results show CALIOP AOD are lower than AERONET AOD especially at low optical depths as measured by AERONET (500nm AOD<0.1). Furthermore, the median relative AOD difference between the two measurements is 25% of the AERONET AOD for AOD>0.1. Differences in AOD between CALIOP and AERONET are possibly due to cloud contamination, scene inhomogeneity, instrument view angle differences, CALIOP retrieval errors, and detection limits. Comparison of daytime to nighttime number of 5km x 60m (60m in the vertical) features detected by CALIOP show that there are 20% more aerosol features at night. We find that CALIPSO and AERONET do not agree on the cloudiness of scenes. Of the scenes that meet the above coincidence criteria, CALIPSO finds clouds in more than 45% of the coincident atmospheric columns AERONET classifies as clear. C1 [Omar, A. H.; Winker, D. M.; Tackett, J. L.; Kar, J.; Liu, Z.; Vaughan, M. A.; Powell, K. A.; Trepte, C. R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Tackett, J. L.; Kar, J.] Sci Syst & Applicat Inc, Hampton, VA USA. [Giles, D. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Giles, D. M.] Sigma Space Corp, Greenbelt, MD USA. [Liu, Z.] Natl Inst Aerosp, Hampton, VA USA. RP Omar, AH (reprint author), NASA, Langley Res Ctr, Sci Directorate, MailStop 475, Hampton, VA 23681 USA. EM ali.h.omar@nasa.gov RI Liu, Zhaoyan/B-1783-2010; Omar, Ali/D-7102-2017 OI Liu, Zhaoyan/0000-0003-4996-5738; Omar, Ali/0000-0003-1871-9235 NR 54 TC 35 Z9 37 U1 6 U2 29 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4748 EP 4766 DI 10.1002/jgrd.50330 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000059 ER PT J AU Meyer, K Platnick, S Oreopoulos, L Lee, DM AF Meyer, Kerry Platnick, Steven Oreopoulos, Lazaros Lee, Dongmin TI Estimating the direct radiative effect of absorbing aerosols overlying marine boundary layer clouds in the southeast Atlantic using MODIS and CALIOP SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE clouds; aerosols; radiative forcing; remote sensing ID CALIPSO LIDAR MEASUREMENTS; OPTICAL-THICKNESS; ALGORITHM; ALBEDO; RETRIEVALS; SCATTERING; PARTICLES; POLLUTION; RADIUS; DEPTH AB Absorbing aerosols such as smoke strongly absorb solar radiation, particularly at ultraviolet and visible/near-infrared (VIS/NIR) wavelengths, and their presence above clouds can have considerable implications. It has been previously shown that they have a positive (i.e., warming) direct aerosol radiative effect (DARE) when overlying bright clouds. Additionally, they can cause biased passive instrument satellite retrievals in techniques that rely on VIS/NIR wavelengths for inferring the cloud optical thickness (COT) and effective radius (r(e)) of underlying clouds, which can in turn yield biased above-cloud DARE estimates. Here we investigate Moderate Resolution Imaging Spectroradiometer (MODIS) cloud optical property retrieval biases due to overlying absorbing aerosols observed by Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) and examine the impact of these biases on above-cloud DARE estimates. The investigation focuses on a region in the southeast Atlantic Ocean during August and September (2006-2011), where smoke from biomass burning in southern Africa overlies persistent marine boundary layer stratocumulus clouds. Adjusting for above-cloud aerosol attenuation yields increases in the regional mean liquid COT (averaged over all ocean-only liquid clouds) by roughly 6%; mean r(e) increases by roughly 2.6%, almost exclusively due to the COT adjustment in the non-orthogonal retrieval space. It is found that these two biases lead to an underestimate of DARE. For liquid cloud Aqua MODIS pixels with CALIOP-observed above-cloud smoke, the regional mean above-cloud radiative forcing efficiency (DARE per unit aerosol optical depth (AOD)) at time of observation (near local noon for Aqua overpass) increases from 50.9Wm(-2)AOD(-1) to 65.1Wm(-2)AOD(-1) when using bias-adjusted instead of nonadjusted MODIS cloud retrievals. C1 [Meyer, Kerry; Lee, Dongmin] Univ Space Res Assoc, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD USA. [Meyer, Kerry; Platnick, Steven; Oreopoulos, Lazaros; Lee, Dongmin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Meyer, K (reprint author), NASA, Goddard Space Flight Ctr, Code 613-0, Greenbelt, MD 20771 USA. EM kerry.meyer@nasa.gov RI Oreopoulos, Lazaros/E-5868-2012; Platnick, Steven/J-9982-2014; Meyer, Kerry/E-8095-2016 OI Oreopoulos, Lazaros/0000-0001-6061-6905; Platnick, Steven/0000-0003-3964-3567; Meyer, Kerry/0000-0001-5361-9200 FU NASA Radiation Sciences Program FX The authors would like to thank Nandana Amarasinghe for his efforts to construct the cloud retrieval look-up tables and Gala Wind for her extensive work on the development of the MOD06 Collection 6 algorithm. In addition, the authors wish to thank Zhibo Zhang for his generous intellectual support during the course of this work and Rob Levy for his assistance with the aerosol component. The MODIS data used in this study were acquired as part of the NASA's Earth-Sun System Division and archived and distributed by the MODIS Adaptive Processing System (MODAPS); CALIOP data were obtained from the NASA Langley Research Center Atmospheric Science Data Center. This research was supported by the NASA Radiation Sciences Program. NR 50 TC 23 Z9 23 U1 4 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4801 EP 4815 DI 10.1002/jgrd.50449 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000063 ER PT J AU Guerlet, S Butz, A Schepers, D Basu, S Hasekamp, OP Kuze, A Yokota, T Blavier, JF Deutscher, NM Griffith, DWT Hase, F Kyro, E Morino, I Sherlock, V Sussmann, R Galli, A Aben, I AF Guerlet, S. Butz, A. Schepers, D. Basu, S. Hasekamp, O. P. Kuze, A. Yokota, T. Blavier, J. -F. Deutscher, N. M. Griffith, D. W. T. Hase, F. Kyro, E. Morino, I. Sherlock, V. Sussmann, R. Galli, A. Aben, I. TI Impact of aerosol and thin cirrus on retrieving and validating XCO2 from GOSAT shortwave infrared measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Remote sensing; Carbon Dioxide; GOSAT; TCCON ID GASES OBSERVING SATELLITE; REFLECTED SUNLIGHT; ATMOSPHERIC CO2; COLUMN; ALGORITHM; SPACE; CARBONTRACKER; CALIBRATION; NETWORK; CLOUDS AB Inadequate treatment of aerosol scattering can be a significant source of error when retrieving column-averaged dry-air mole fractions of CO2 (XCO2) from space-based measurements of backscattered solar shortwave radiation. We have developed a retrieval algorithm, RemoTeC, that retrieves three aerosol parameters (amount, size, and height) simultaneously with XCO2. Here we evaluate the ability of RemoTeC to account for light path modifications by clouds, subvisual cirrus, and aerosols when retrieving XCO2 from Greenhouse Gases Observing Satellite (GOSAT) Thermal and Near-infrared Sensor for carbon Observation (TANSO)-Fourier Transform Spectrometer (FTS) measurements. We first evaluate a cloud filter based on measurements from the Cloud and Aerosol Imager and a cirrus filter that uses radiances measured by TANSO-FTS in the 2micron spectral region, with strong water absorption. For the cloud-screened scenes, we then evaluate errors due to aerosols. We find that RemoTeC is well capable of accounting for scattering by aerosols for values of aerosol optical thickness at 750nm up to 0.25. While no significant correlation of errors is found with albedo, correlations are found with retrieved aerosol parameters. To further improve the XCO2 accuracy, we propose and evaluate a bias correction scheme. Measurements from 12 ground-based stations of the Total Carbon Column Observing Network (TCCON) are used as a reference in this study. We show that spatial colocation criteria may be relaxed using additional constraints based on modeled XCO2 gradients, to increase the size and diversity of validation data and provide a more robust evaluation of GOSAT retrievals. Global-scale validation of satellite data remains challenging and would be improved by increasing TCCON coverage. C1 [Guerlet, S.; Schepers, D.; Basu, S.; Hasekamp, O. P.; Galli, A.; Aben, I.] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Guerlet, S.] UPMC, CNRS, IPSL, Lab Meteorol Dynam, F-75252 Paris, France. [Butz, A.; Hase, F.] Karlsruhe Inst Technol, IMK ASF, Eggenstein Leopoldshafen, Germany. [Kuze, A.] Japanese Aerosp Explorat Agcy JAXA, Tsukuba, Ibaraki, Japan. [Yokota, T.; Morino, I.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Blavier, J. -F.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Deutscher, N. M.] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. [Deutscher, N. M.; Griffith, D. W. T.] Univ Wollongong, Sch Chem, Wollongong, NSW, Australia. [Kyro, E.] Finnish Meteorol Inst, Arctic Res Ctr, FIN-00101 Helsinki, Finland. [Sherlock, V.] Natl Inst Water & Atmospher Res, Wellington, New Zealand. [Sussmann, R.] Karlsruhe Inst Technol, IMK IFU, Garmisch Partenkirchen, Germany. RP Guerlet, S (reprint author), UPMC, CNRS, IPSL, Lab Meteorol Dynam, 4 Pl Jussieu, F-75252 Paris, France. EM sandrine.guerlet@lmd.jussieu.fr RI Butz, Andre/A-7024-2013; Garmisch-Pa, Ifu/H-9902-2014; Morino, Isamu/K-1033-2014; Deutscher, Nicholas/E-3683-2015; KUZE, AKIHIKO/J-2074-2016; Sussmann, Ralf/K-3999-2012 OI Butz, Andre/0000-0003-0593-1608; Morino, Isamu/0000-0003-2720-1569; Deutscher, Nicholas/0000-0002-2906-2577; KUZE, AKIHIKO/0000-0001-5415-3377; FU ESA's Climate Change Initiative on GHGs; European Commission [218793]; Emmy-Noether programme of Deutsche Forschungsgemeinschaft (DFG) [BU2599/1-1]; Dutch User Support Program [GO-AO/21]; Gebruikersondersteuning ruimteonderzoek program of the Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO) [ALW-GO-AO/08-10]; NASA's Terrestrial Ecology Program [NNX11AG01G]; Orbiting Carbon Observatory Program; Atmospheric CO2 Observations from Space (ACOS) Program; DOE/ARM Program; National Aeronautics and Space Administration; OCO project; OCO-2 project; Australian Research Council [LE0668470, DP0879468, DP110103118, LP0562346]; New Zealand Foundation of Research Science and Technology [C01X0204, CO1X0406]; ESA; University of Bremen; EC within the INGOS project; Senate of Bremen FX Access to GOSAT data was granted through the second GOSAT research announcement jointly issued by JAXA, NIES, and MOE. SG acknowledges funding from ESA's Climate Change Initiative on GHGs and the European Commission's seventh framework program under grant agreement 218793. AB is supported by the Emmy-Noether programme of Deutsche Forschungsgemeinschaft (DFG) through grant BU2599/1-1 (RemoTeC). DS is funded by the Dutch User Support Program under project GO-AO/21. SB was supported by the Gebruikersondersteuning ruimteonderzoek program of the Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO) through project ALW-GO-AO/08-10. We wish to thank Jean-Michel Hartmann and Ha Tran for providing line-mixing parameters. CarbonTracker 2010 results were provided by NOAA ESRL, Boulder, Colorado, USA from the website at http://carbontracker.noaa.gov. TCCON data were obtained from the TCCON Data Archive, operated by the California Institute of Technology from the website at http://tccon.ipac.caltech.edu/. U.S. funding for TCCON comes from NASA's Terrestrial Ecology Program, grant NNX11AG01G, the Orbiting Carbon Observatory Program, the Atmospheric CO2 Observations from Space (ACOS) Program and the DOE/ARM Program. Some of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The Darwin TCCON site was built at Caltech with funding from the OCO project and is operated by the University of Wollongong, with travel funds for maintenance and equipment costs funded by the OCO-2 project. We acknowledge funding to support Darwin and Wollongong from the Australian Research Council, Projects LE0668470, DP0879468, DP110103118, and LP0562346. Lauder TCCON measurements are funded by New Zealand Foundation of Research Science and Technology contracts C01X0204 and CO1X0406. The Garmisch TCCON team acknowledges funding by ESA (GHG-CCI project via subcontract with University of Bremen) and by the EC within the INGOS project. We acknowledge financial support of the Bialystok and Orleans TCCON sites from the Senate of Bremen and EU projects IMECC and Geomon as well as maintenance and logistical work provided by AeroMeteo Service (Bialystok) and the RAMCES team at LSCE (Gif-sur-Yvette, France). NR 33 TC 33 Z9 34 U1 1 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4887 EP 4905 DI 10.1002/jgrd.50332 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000069 ER PT J AU Guo, YJ Tian, BJ Kahn, RA Kalashnikova, O Wong, S Waliser, DE AF Guo, Yanjuan Tian, Baijun Kahn, Ralph A. Kalashnikova, Olga Wong, Sun Waliser, Duane E. TI Tropical Atlantic dust and smoke aerosol variations related to the Madden-Julian Oscillation in MODIS and MISR observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol; dust; smoke; MJO; satellite; Atlantic ID REMOTE-SENSING OBSERVATIONS; OPTICAL-THICKNESS; IMAGING SPECTRORADIOMETER; SIZE DISTRIBUTION; OCEAN; SENSITIVITY; RETRIEVALS; PRODUCTS; REANALYSIS; IDENTIFY AB In this study, Moderate Resolution Imaging Spectroradiometer (MODIS) fine mode fraction and Multi-angle Imaging SpectroRadiometer (MISR) nonspherical fraction data are used to derive dust and smoke aerosol optical thickness ((dust) and (smoke)) over the tropical Atlantic in a complementary way: due to its wider swath, MODIS has 3-4 times greater sampling than MISR, but MISR dust discrimination is based on particle shape retrievals, whereas an empirical scheme is used for MODIS. MODIS and MISR show very similar dust and smoke winter climatologies. (dust) is the dominant aerosol component over the tropical Atlantic, accounting for 40-70% of the total aerosol optical thickness (AOT), whereas (smoke) is significantly smaller than (dust). The consistency and high correlation between these climatologies and their daily variations lends confidence to their use for investigating the relative dust and smoke contributions to the total AOT variation associated with the Madden-Julian Oscillation (MJO). The temporal evolution and spatial patterns of the (dus) anomalies associated with the MJO are consistent between MODIS and MISR: the magnitude of MJO-realted (dust) anomalies is comparable to or even larger than that of the total , while the (smoke) anomaly represents about 15% compared to the total, which is quite different from their relative magnitudes to the total on the climatological time scale. This suggests that dust and smoke are not influenced by the MJO in the same way. Based on correlation analysis, dust is strongly influenced by the MJO-modulated trade wind and precipitation anomalies, and can last as long as one MJO phase, whereas smoke is less affected. C1 [Guo, Yanjuan; Tian, Baijun; Kalashnikova, Olga; Wong, Sun; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Guo, Yanjuan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Kahn, Ralph A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tian, BJ (reprint author), CALTECH, Jet Prop Lab, M-S 233-304,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM baijun.tian@jpl.nasa.gov RI Tian, Baijun/A-1141-2007; Kahn, Ralph/D-5371-2012 OI Tian, Baijun/0000-0001-9369-2373; Kahn, Ralph/0000-0002-5234-6359 FU National Science Foundation (NSF) University of California, Los Angeles [ATM-0840755]; NASA's Climate and Radiation Research and Analysis Program; EOS-MISR project; NASA's Atmospheric Composition Program FX This research was performed at Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under a contract with National Aeronautics and Space Administration (NASA). It was supported in part by the National Science Foundation (NSF) grant ATM-0840755 at University of California, Los Angeles. The work of R. Kahn is supported in part by NASA's Climate and Radiation Research and Analysis Program, under H. Maring, NASA's Atmospheric Composition Program under R. Eckman, and the EOS-MISR project. The MODIS/Aqua data used in this study have been obtained from the NASA LAADS server and ERA-Interim data used in this study have been obtained from the ECMWF Data Server. (C) 2011. All rights reserved. NR 48 TC 11 Z9 11 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 27 PY 2013 VL 118 IS 10 BP 4947 EP 4963 DI 10.1002/jgrd.50409 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229NB UT WOS:000325272000073 ER PT J AU Toller, G Xiong, XX Sun, JQ Wenny, BN Geng, X Kuyper, J Angal, A Chen, HD Madhavan, S Wua, AS AF Toller, Gary Xiong, Xiaoxiong Sun, Junqiang Wenny, Brian N. Geng, Xu Kuyper, James Angal, Amit Chen, Hongda Madhavan, Sriharsha Wua, Aisheng TI Terra and Aqua moderate-resolution imaging spectroradiometer collection 6 level 1B algorithm SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE moderate-resolution imaging spectroradiometer; Terra; Aqua; remote sensing; data processing; satellite ID REFLECTIVE SOLAR BANDS; ON-ORBIT CALIBRATION; MODIS; PERFORMANCE AB The moderate-resolution imaging spectroradiometer (MODIS) was launched on the Terra spacecraft on Dec. 18, 1999 and on Aquaon May 4, 2002. The data acquired by these instruments have contributed to the long-term climate data record for more than a decade and represent a key component of NASA's Earth observing system. Each MODIS instrument observes nearly the whole Earth each day, enabling the scientific characterization of the land, ocean, and atmosphere. The MODIS Level 1B (L1B) algorithms input uncalibrated geo-located observations and convert instrument response into calibrated reflectance and radiance, which are used to generate science data products. The instrument characterization needed to run the L1B code is currently implemented using time-dependent lookup tables. The MODIS characterization support team, working closely with the MODIS Science Team, has improved the product quality with each data reprocessing. We provide an overview of the new L1B algorithm release, designated collection 6. Recent improvements made as a consequence of on-orbit calibration, onorbit analyses, and operational considerations are described. Instrument performance and the expected impact of L1B changes on the collection 6 L1B products are discussed. (C) 2013 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Toller, Gary; Sun, Junqiang; Wenny, Brian N.; Geng, Xu; Kuyper, James; Chen, Hongda; Wua, Aisheng] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. [Angal, Amit; Madhavan, Sriharsha] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Toller, G (reprint author), Sigma Space Corp, 4801 Forbes Blvd, Lanham, MD 20706 USA. EM gtoller@sigmaspace.com NR 29 TC 13 Z9 13 U1 0 U2 15 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD MAY 22 PY 2013 VL 7 AR 073557 DI 10.1117/1.JRS.7.073557 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 151YU UT WOS:000319497100001 ER PT J AU Schmidt, R Tantoyotai, P Fakra, SC Marcus, MA Yang, SI Pickering, IJ Banuelos, GS Hristova, KR Freeman, JL AF Schmidt, Radomir Tantoyotai, Prapakorn Fakra, Sirine C. Marcus, Matthew A. Yang, Soo In Pickering, Ingrid J. Banuelos, Gary S. Hristova, Krassimira R. Freeman, John L. TI Selenium Biotransformations in an Engineered Aquatic Ecosystem for Bioremediation of Agricultural Wastewater via Brine Shrimp Production SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID RAY-ABSORPTION SPECTROSCOPY; EPHYDRA-CINEREA JONES; GREAT-SALT-LAKE; DRAINAGE SEDIMENT; SPECIATION; CALIFORNIA; SELENATE; ACCUMULATION; ORGANISMS; TOXICITY AB An engineered aquatic ecosystem was specifically designed to bioremediate selenium (Se), occurring as oxidized inorganic selenate from hypersalinized agricultural drainage water while producing brine shrimp enriched in organic Se and omega-3 and omega-6 fatty acids for use in value added nutraceutical food supplements. Selenate was successfully bioremediated by microalgal metabolism into organic Se (seleno-amino acids) and partially removed via gaseous volatile Se formation. Furthermore, filter feeding brine shrimp that accumulated this organic Se were removed by net harvest. Thriving in this engineered pond system, brine shrimp (Artemia franciscana Kellogg) and brine fly (Ephydridae sp.) have major ecological relevance as important food sources for large populations of waterfowl, breeding, and migratory shore birds. This aquatic ecosystem was an ideal model for study because it mimics trophic interactions in a Se polluted wetland. Inorganic selenate in drainage water was metabolized differently in microalgae, bacteria, and diatoms where it was accumulated and reduced into various inorganic forms (selenite, selenide, or elemental Se) or partially incorporated into organic Se mainly as selenomethionine. Brine shrimp and brine fly larva then bioaccumulated Se from ingesting aquatic microorganisms and further metabolized Se predominately into organic Se forms. Importantly, adult brine flies, which hatched from aquatic larva, bioaccumulated the highest Se concentrations of all organisms tested. C1 [Schmidt, Radomir; Tantoyotai, Prapakorn; Hristova, Krassimira R.] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Fakra, Sirine C.; Marcus, Matthew A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Yang, Soo In; Pickering, Ingrid J.] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. [Banuelos, Gary S.] ARS, USDA, SJVASC, Water Management Res Div, Parlier, CA 93648 USA. [Hristova, Krassimira R.] Marquette Univ, Dept Sci Biol, Milwaukee, WI 53233 USA. [Freeman, John L.] Calif State Univ Fresno, Dept Biol, Fresno, CA 93740 USA. [Freeman, John L.] NASA, Ames Res Ctr, Intrinsyx Technol Corp Inc, Space Biosci Div, Moffett Field, CA 94035 USA. RP Hristova, KR (reprint author), Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. EM krassimira.hristova@marquette.edu; John.L.Freeman@NASA.gov RI Pickering, Ingrid/A-4547-2013 FU CSU Fresno California Agricultural Research Initiative; Department of Energy; California Department of Water Resources [08-002104, 07-3]; Office of Science, Office of Basic Energy Sciences, U.S. Department of Energy [DE-AC02-05CH11231]; DOE, Office of Biological and Environmental Research; National Institutes of Health, National Center for Research Resources, Biomedical Technology Program [P41RR001209]; Natural Sciences and Engineering Research Council of Canada; CIHR-THRUST Fellowship FX This research was supported by a CSU Fresno California Agricultural Research Initiative granted to Dr. Gary S. Banuelos and Dr. John L. Freeman, a Department of Energy Beam Time grant to Dr. Gary S. Banuelos and Dr. John L Freeman, and by the California Department of Water Resources under contract number 08-002104, task order 07-3, granted to Dr. Krassimira R. Hristova. The operations of the Advanced Light Source at Lawrence Berkeley National Laboratory were supported by the Director, Office of Science, Office of Basic Energy Sciences, U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The Stanford Synchrotron Radiation Lightsource (SSRL), a Directorate of SLAC National Accelerator Laboratory and an Office of Science User Facility is operated for the U.S. Department of Energy Office of Science by Stanford University. The SSRL Structural Molecular Biology Program is supported by the DOE, Office of Biological and Environmental Research, and by the National Institutes of Health, National Center for Research Resources, Biomedical Technology Program (P41RR001209). Ingrid J. Pickering is a Canada Research Chair and Soo In Yang was funded by the Natural Sciences and Engineering Research Council of Canada (Discovery Grant to IJP) and by a CIHR-THRUST Fellowship. NR 59 TC 5 Z9 5 U1 3 U2 60 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD MAY 21 PY 2013 VL 47 IS 10 BP 5057 EP 5065 DI 10.1021/es305001n PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 154WY UT WOS:000319708600013 PM 23621086 ER PT J AU Hosking, SG Davey, CE Kaiser, MK AF Hosking, Simon G. Davey, Catherine E. Kaiser, Mary K. TI Visual cues for manual control of headway SO FRONTIERS IN BEHAVIORAL NEUROSCIENCE LA English DT Article DE visual perception; manual control; headway regulation; optic cues; control dynamics ID TIME-TO-COLLISION; OPTICAL INFORMATION; BRAKING; PERCEPTION; MOTION; SPEED; TAU; ACCELERATION; CONTACT; JUDGMENTS AB The ability to maintain appropriate gaps to objects in one's environment is important when navigating through a three-dimensional world. Previous research has shown that the visual angle subtended by a lead/approaching object and its rate of change are important variables for timing interceptions, collision avoidance, continuous regulation of braking, and manual control of headway. However, investigations of headway maintenance have required participants to maintain a fixed distance headway and have not investigated how information about own-speed is taken into account. In the following experiment, we asked participants to use a joystick to follow computer-simulated lead objects. The results showed that ground texture, following speed, and the size of the lead object had significant effects on both mean following distances and following distance variance. Furthermore, models of the participants' joystick responses provided better fits when it was assumed that the desired visual extent of the lead object would vary over time. Taken together, the results indicate that while information about own-speed is used by controllers to set the desired headway to a lead object, the continuous regulation of headway is influenced primarily by the visual angle of the lead object and its rate of change. The reliance on visual angle, its rate of change, and/or own-speed information also varied depending on the control dynamics of the system. Such findings are consistent with an optimal control criterion that reflects a differential weighting on different sources of information depending on the plant dynamics. As in other judgements of motion in depth, the information used for controlling headway to other objects in the environment varies depending on the constraints of the task and different strategies of control. C1 [Hosking, Simon G.; Davey, Catherine E.] Def Sci & Technol Org, Air Operat Div, Fishermans Bend, Vic 3207, Australia. [Kaiser, Mary K.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. RP Hosking, SG (reprint author), Def Sci & Technol Org, Air Operat Div, 506 Lorimer St, Fishermans Bend, Vic 3207, Australia. EM simon.hosking@dsto.defence.gov.au OI DAVEY, CATHERINE/0000-0002-5672-7941 NR 37 TC 0 Z9 0 U1 0 U2 7 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1662-5153 J9 FRONT BEHAV NEUROSCI JI Front. Behav. Neurosci. PD MAY 21 PY 2013 VL 7 AR 45 DI 10.3389/fnbeh.2013.00045 PG 14 WC Behavioral Sciences; Neurosciences SC Behavioral Sciences; Neurosciences & Neurology GA 149MD UT WOS:000319323100001 PM 23750130 ER PT J AU Moscatelli, F Marisaldi, M Maccagnani, P Labanti, C Fuschino, F Prest, M Berra, A Bolognini, D Ghioni, M Rech, I Gulinatti, A Giudice, A Simmerle, G Candelori, A Mattiazzo, S Sun, XL Cavanaugh, JF Rubini, D AF Moscatelli, Francesco Marisaldi, Martino Maccagnani, Piera Labanti, Claudio Fuschino, Fabio Prest, Michela Berra, Alessandro Bolognini, Davide Ghioni, Massimo Rech, Ivan Gulinatti, Angelo Giudice, Andrea Simmerle, Georg Candelori, Andrea Mattiazzo, Serena Sun, Xiaoli Cavanaugh, John F. Rubini, Danilo TI Radiation tests of single photon avalanche diode for space applications SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Single photon detection; Radiation hardness; Space-qualified detectors ID LEVEL TRANSIENT SPECTROSCOPY; HIGH-RESISTIVITY SILICON; IRRADIATION FACILITY; NEUTRON-IRRADIATION; PROTON IRRADIATION; DAMAGE; DETECTORS; PHOTODIODES; DEFECTS; CIRCUIT AB Single photon avalanche diodes (SPADs) have been recently studied as photodetectors for applications in space missions. In this presentation we report the results of radiation hardness test on large area SPAD (actual results refer to SPADs having 500 mu m diameter). Dark counts rate as low as few kHz at -10 degrees C has been obtained for the 500 mu m devices, before irradiation. We performed bulk damage and total dose radiation tests with protons and gamma-rays in order to evaluate their radiation hardness properties and their suitability for application in a Low Earth Orbit (LEO) space mission. With this aim SPAD devices have been irradiated using up to 20 krad total dose with gamma-rays and 5 krad with protons. The test performed show that large area SPADs are very sensitive to proton doses as low as 2 x 10(8) (1 MeV eq) n/cm(2) with a significant increase in dark counts rate (DCR) as well as in the manifestation of the "random telegraph signal" effect. Annealing studies at room temperature (RT) and at 80 degrees C have been carried out, showing a high decrease of DCR after 24-48 h at RT. Lower protons doses in the range 1-10 x 10(7) (1 MeV eq) n/cm(2) result in a lower increase of DCR suggesting that the large-area SPADs tested in this study are well suitable for application in low-inclination LEO, particularly useful for gamma-ray astrophysics. (c) 2013 Elsevier B.V. All rights reserved. C1 [Moscatelli, Francesco; Maccagnani, Piera] CNR IMM Bologna, I-40129 Bologna, Italy. [Marisaldi, Martino; Labanti, Claudio; Fuschino, Fabio] INAF IASF Bologna, I-40129 Bologna, Italy. [Prest, Michela; Berra, Alessandro; Bolognini, Davide] Univ Insubria, I-22100 Como, Italy. [Prest, Michela; Berra, Alessandro; Bolognini, Davide] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-22100 Como, Italy. [Ghioni, Massimo; Rech, Ivan; Gulinatti, Angelo] Politecn Milan, Dipartimento Elettron & Informaz, I-20133 Milan, Italy. [Giudice, Andrea; Simmerle, Georg] Micro Photon Devices, I-39100 Bolzano, Italy. [Candelori, Andrea; Mattiazzo, Serena] Univ Padua, Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Candelori, Andrea; Mattiazzo, Serena] Univ Padua, Dipartimento Fis, I-35131 Padua, Italy. [Sun, Xiaoli; Cavanaugh, John F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rubini, Danilo] Italian Space Agcy, I-00198 Rome, Italy. RP Moscatelli, F (reprint author), CNR IMM Bologna, Via Gobetti 101, I-40129 Bologna, Italy. EM moscatelli@bo.imm.cnr.it RI Sun, Xiaoli/B-5120-2013; GULINATTI, ANGELO/F-1335-2010; maccagnani, piera/H-6428-2014; Moscatelli, Francesco/N-6333-2014; OI GULINATTI, ANGELO/0000-0001-6701-9126; Berra, Alessandro/0000-0002-9031-4585; Labanti, Claudio/0000-0002-5086-3619; maccagnani, piera/0000-0003-0288-0219; Moscatelli, Francesco/0000-0002-7676-3106; Fuschino, Fabio/0000-0003-2139-3299; PREST, MICHELA/0000-0003-3161-4454; Marisaldi, Martino/0000-0002-4000-3789; Rech, Ivan/0000-0002-1430-1010 FU Italian Space Agency (ASI) [I/039/09/0] FX This work was carried out under the Italian Space Agency (ASI) Contract I/039/09/0. The authors wish to thank the staff of Sant'Anna Hospital, Como, the staff of PSI of Zurich and INFN Laboratori Nazionali di Legnaro for their support during the irradiation tests. NR 36 TC 3 Z9 3 U1 2 U2 20 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 MAY 21 PY 2013 VL 711 BP 65 EP 72 DI 10.1016/j.nima.2013.01.056 PG 8 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 135WL UT WOS:000318321300009 ER PT J AU Ashby, MLN Willner, SP Fazio, GG Huang, JS Arendt, R Barmby, P Barro, G Bell, EF Bouwens, R Cattaneo, A Croton, D Dave, R Dunlop, JS Egami, E Faber, S Finlator, K Grogin, NA Guhathakurta, P Hernquist, L Hora, JL Illingworth, G Kashlinsky, A Koekemoer, AM Koo, DC Labbe, I Li, Y Lin, L Moseley, H Nandra, K Newman, J Noeske, K Ouchi, M Peth, M Rigopoulou, D Robertson, B Sarajedini, V Simard, L Smith, HA Wang, Z Wechsler, R Weiner, B Wilson, G Wuyts, S Yamada, T Yan, H AF Ashby, M. L. N. Willner, S. P. Fazio, G. G. Huang, J. -S. Arendt, R. Barmby, P. Barro, G. Bell, E. F. Bouwens, R. Cattaneo, A. Croton, D. Dave, R. Dunlop, J. S. Egami, E. Faber, S. Finlator, K. Grogin, N. A. Guhathakurta, P. Hernquist, L. Hora, J. L. Illingworth, G. Kashlinsky, A. Koekemoer, A. M. Koo, D. C. Labbe, I. Li, Y. Lin, L. Moseley, H. Nandra, K. Newman, J. Noeske, K. Ouchi, M. Peth, M. Rigopoulou, D. Robertson, B. Sarajedini, V. Simard, L. Smith, H. A. Wang, Z. Wechsler, R. Weiner, B. Wilson, G. Wuyts, S. Yamada, T. Yan, H. TI SEDS: THE SPITZER EXTENDED DEEP SURVEY. SURVEY DESIGN, PHOTOMETRY, AND DEEP IRAC SOURCE COUNTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; infrared: galaxies; surveys ID EXTRAGALACTIC LEGACY SURVEY; LYMAN-BREAK GALAXIES; INFRARED BACKGROUND FLUCTUATIONS; SPACE-TELESCOPE OBSERVATIONS; UV LUMINOSITY FUNCTIONS; STAR-FORMATION HISTORY; EXTREMELY RED OBJECTS; CLUSTERING PROPERTIES; REDSHIFT SURVEY; MU-M AB The Spitzer Extended Deep Survey (SEDS) is a very deep infrared survey within five well-known extragalactic science fields: the UKIDSS Ultra-Deep Survey, the Extended Chandra Deep Field South, COSMOS, the Hubble Deep Field North, and the Extended Groth Strip. SEDS covers a total area of 1.46 deg(2) to a depth of 26 AB mag (3s) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5 mu m. Because of its uniform depth of coverage in so many widely-separated fields, SEDS is subject to roughly 25% smaller errors due to cosmic variance than a single-field survey of the same size. SEDS was designed to detect and characterize galaxies from intermediate to high redshifts (z = 2-7) with a built-in means of assessing the impact of cosmic variance on the individual fields. Because the full SEDS depth was accumulated in at least three separate visits to each field, typically with six- month intervals between visits, SEDS also furnishes an opportunity to assess the infrared variability of faint objects. This paper describes the SEDS survey design, processing, and publicly-available data products. Deep IRAC counts for the more than 300,000 galaxies detected by SEDS are consistent with models based on known galaxy populations. Discrete IRAC sources contribute 5.6 +/- 1.0 and 4.4 +/- 0.8 nW m(-2) sr(-1) at 3.6 and 4.5 mu m to the diffuse cosmic infrared background (CIB). IRAC sources cannot contribute more than half of the total CIB flux estimated from DIRBE data. Barring an unexpected error in the DIRBE flux estimates, half the CIB flux must therefore come from a diffuse component. C1 [Ashby, M. L. N.; Willner, S. P.; Fazio, G. G.; Huang, J. -S.; Hernquist, L.; Hora, J. L.; Smith, H. A.; Wang, Z.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arendt, R.; Kashlinsky, A.; Moseley, H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Arendt, R.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Barmby, P.] Univ Western Ontario, London, ON N6A 3K7, Canada. [Barro, G.; Faber, S.; Guhathakurta, P.; Illingworth, G.; Koo, D. C.] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Barro, G.; Faber, S.; Guhathakurta, P.; Illingworth, G.; Koo, D. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bouwens, R.; Labbe, I.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Cattaneo, A.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Croton, D.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Dave, R.; Robertson, B.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Dunlop, J. S.] Univ Edinburgh, Royal Observ, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland. [Egami, E.; Robertson, B.; Weiner, B.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Finlator, K.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Grogin, N. A.; Koekemoer, A. M.; Noeske, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kashlinsky, A.] SSAI, Lanham, MD 20706 USA. [Li, Y.] Penn State Univ, Dept Phys & Astron, University Pk, PA 16802 USA. [Li, Y.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Lin, L.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Nandra, K.; Wuyts, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Newman, J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Ouchi, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Ouchi, M.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Peth, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England. [Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Sarajedini, V.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Simard, L.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC, Canada. [Wechsler, R.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Wechsler, R.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Wilson, G.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 980, Japan. [Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mashby@cfa.harvard.edu RI Finlator, Kristian/M-4809-2014; Barmby, Pauline/I-7194-2016 OI Finlator, Kristian/0000-0002-0496-1656; Hora, Joseph/0000-0002-5599-4650; Koekemoer, Anton/0000-0002-6610-2048; Arendt, Richard/0000-0001-8403-8548; Bell, Eric/0000-0002-5564-9873; Barmby, Pauline/0000-0003-2767-0090 FU National Aeronautics and Space Administration (NASA); NASA [1367335, 1367411, 1367412]; European Research Council; Royal Society via a Wolfson Research Merit Award; National Science Foundation FX The authors are grateful to E. Diolaiti for helpful advice on the optimal use of StarFinder. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through contract numbers 1367335, 1367411 and 1367412 issued by JPL/Caltech. J.S.D. acknowledges the support of the European Research Council via an Advanced Grant, and the support of the Royal Society via a Wolfson Research Merit Award. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. NR 69 TC 83 Z9 83 U1 2 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 MAY 20 PY 2013 VL 769 IS 1 AR 80 DI 10.1088/0004-637X/769/1/80 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500080 ER PT J AU Cappelluti, N Kashlinsky, A Arendt, RG Comastri, A Fazio, GG Finoguenov, A Hasinger, G Mather, JC Miyaji, T Moseley, SH AF Cappelluti, N. Kashlinsky, A. Arendt, R. G. Comastri, A. Fazio, G. G. Finoguenov, A. Hasinger, G. Mather, J. C. Miyaji, T. Moseley, S. H. TI CROSS-CORRELATING COSMIC INFRARED AND X-RAY BACKGROUND FLUCTUATIONS: EVIDENCE OF SIGNIFICANT BLACK HOLE POPULATIONS AMONG THE CIB SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; infrared: diffuse background; stars: Population III; X-rays: diffuse background ID ACTIVE GALACTIC NUCLEI; COBE DIRBE MAPS; SPITZER-SPACE-TELESCOPE; WIDE-FIELD SURVEY; ALL-SKY SURVEY; NUMBER COUNTS; SOURCE CATALOG; POWER SPECTRUM; GOODS FIELDS; III STARS AB In order to understand the nature of the sources producing the recently uncovered cosmic infrared background (CIB) fluctuations, we study cross-correlations between the fluctuations in the source-subtracted CIB from Spitzer/IRAC data and the unresolved cosmic X-ray background from deep Chandra observations. Our study uses data from the EGS/AEGIS field, where both data sets cover an similar or equal to 8' x 45' region of the sky. Our measurement is the cross-power spectrum between the IR and X-ray data. The cross-power signal between the IRAC maps at 3.6 mu m and 4.5 mu m and the Chandra [0.5-2] keV data has been detected, at angular scales greater than or similar to 20 '', with an overall significance of similar or equal to 3.8 sigma and similar or equal to 5.6 sigma, respectively. At the same time we find no evidence of significant cross-correlations at the harder Chandra bands. The cross-correlation signal is produced by individual IR sources with 3.6 mu m and 4.5 mu m magnitudes m(AB) greater than or similar to 25-26 and [0.5-2] keV X-ray fluxes << 7 x 10(-17) erg cm(2) s(-1). We determine that at least 15%-25% of the large scale power of the CIB fluctuations is correlated with the spatial power spectrum of the X-ray fluctuations. If this correlation is attributed to emission from accretion processes at both IR and X-ray wavelengths, this implies a much higher fraction of accreting black holes than among the known populations. We discuss the various possible origins for the cross-power signal and show that neither local foregrounds nor the known remaining normal galaxies and active galactic nuclei can reproduce the measurements. These observational results are an important new constraint on theoretical modeling of the near-IR CIB fluctuations. C1 [Cappelluti, N.; Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Cappelluti, N.; Arendt, R. G.; Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Kashlinsky, A.; Arendt, R. G.; Mather, J. C.; Moseley, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Kashlinsky, A.] SSAI, Lanham, MD 20706 USA. [Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finoguenov, A.] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland. [Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Mather, J. C.; Moseley, S. H.] NASA, Greenbelt, MD 20771 USA. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, BC, Mexico. RP Cappelluti, N (reprint author), INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. RI Comastri, Andrea/O-9543-2015; OI Comastri, Andrea/0000-0003-3451-9970; Cappelluti, Nico/0000-0002-1697-186X; Arendt, Richard/0000-0001-8403-8548 FU NASA Chandra Archival research grant [AR2-13014B]; INAF fellowship program; Della Riccia foundation; [ASI-INAFI/009/10/0] FX N.C., A.K., and R.A. acknowledge NASA Chandra Archival research grant No. AR2-13014B for partial support. N.C. acknowledges the INAF fellowship program. We acknowledge financial contribution from the agreement ASI-INAFI/009/10/0. N.C. acknowledges the Della Riccia foundation for partially funding this project. NR 57 TC 24 Z9 24 U1 1 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 MAY 20 PY 2013 VL 769 IS 1 AR 68 DI 10.1088/0004-637X/769/1/68 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500068 ER PT J AU Danchi, WC Lopez, B AF Danchi, William C. Lopez, Bruno TI EFFECT OF METALLICITY ON THE EVOLUTION OF THE HABITABLE ZONE FROM THE PRE-MAIN SEQUENCE TO THE ASYMPTOTIC GIANT BRANCH AND THE SEARCH FOR LIFE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars: evolution; stars: late-type; techniques: high angular resolution ID KEPLER PLANETARY CANDIDATES; M-CIRCLE-PLUS; RAPID APPEARANCE; METAZOAN PHYLA; SUPER-EARTHS; RED GIANTS; WIDE-RANGE; EARLY MARS; STARS; MASS AB During the course of stellar evolution, the location and width of the habitable zone changes as the luminosity and radius of the star evolves. The duration of habitability for a planet located at a given distance from a star is greatly affected by the characteristics of the host star. A quantification of these effects can be used observationally in the search for life around nearby stars. The longer the duration of habitability, the more likely it is that life has evolved. The preparation of observational techniques aimed at detecting life would benefit from the scientific requirements deduced from the evolution of the habitable zone. We present a study of the evolution of the habitable zone around stars of 1.0, 1.5, and 2.0 M-circle dot for metallicities ranging from Z = 0.0001 to Z = 0.070. We also consider the evolution of the habitable zone from the pre-main sequence until the asymptotic giant branch is reached. We find that metallicity strongly affects the duration of the habitable zone for a planet as well as the distance from the host star where the duration is maximized. For a 1.0 M-circle dot star with near solar metallicity, Z = 0.017, the duration of the habitable zone is > 10 Gyr at distances 1.2-2.0 AU from the star, whereas the duration is > 20 Gyr for high-metallicity stars (Z = 0.070) at distances of 0.7-1.8 AU, and similar to 4 Gyr at distances of 1.8-3.3 AU for low-metallicity stars (Z = 0.0001). Corresponding results have been obtained for stars of 1.5 and 2.0 solar masses. C1 [Danchi, William C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Lopez, Bruno] Observ Cote Azur, Lab Lagrange UMR 7293, F-06034 Nice 4, France. RP Danchi, WC (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. EM william.c.danchi@nasa.gov; bruno.lopez@oca.eu NR 58 TC 7 Z9 7 U1 0 U2 6 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 MAY 20 PY 2013 VL 769 IS 1 AR 27 DI 10.1088/0004-637X/769/1/27 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500027 ER PT J AU Stewart, KR Brooks, AM Bullock, JS Maller, AH Diemand, J Wadsley, J Moustakas, LA AF Stewart, Kyle R. Brooks, Alyson M. Bullock, James S. Maller, Ariyeh H. Diemand, Juerg Wadsley, James Moustakas, Leonidas A. TI ANGULAR MOMENTUM ACQUISITION IN GALAXY HALOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: halos; galaxies: kinematics and dynamics; intergalactic medium; methods: numerical ID DARK-MATTER HALOES; ACTIVE GALACTIC NUCLEI; TIDAL-TORQUE THEORY; EDGE-ON GALAXIES; DISK GALAXIES; BLACK-HOLES; COSMOLOGICAL SIMULATIONS; HIGH-REDSHIFT; COSMIC GAS; COLD FLOWS AB We use high-resolution cosmological hydrodynamic simulations to study the angular momentum acquisition of gaseous halos around Milky-Way-sized galaxies. We find that cold mode accreted gas enters a galaxy halo with similar to 70% more specific angular momentum than dark matter averaged over cosmic time ( though with a very large dispersion). In fact, we find that all matter has a higher spin parameter when measured at accretion than when averaged over the entire halo lifetime, and is well characterized by. lambda similar to 0.1, at accretion. Combined with the fact that cold flow gas spends a relatively short time (1-2 dynamical times) in the halo before sinking to the center, this naturally explains why cold flow halo gas has a specific angular momentum much higher than that of the halo and often forms "cold flow disks." We demonstrate that the higher angular momentum of cold flow gas is related to the fact that it tends to be accreted along filaments. C1 [Stewart, Kyle R.] Calif Baptist Univ, Dept Nat & Math Sci, Riverside, CA 92504 USA. [Stewart, Kyle R.; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brooks, Alyson M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Bullock, James S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [Bullock, James S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA. [Maller, Ariyeh H.] New York City Coll Technol, Dept Phys, Brooklyn, NY 11201 USA. [Diemand, Juerg] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Wadsley, James] McMaster Univ, Dept Phys & Astron, Hamilton L85 4M1, ON, Canada. RP Stewart, KR (reprint author), Calif Baptist Univ, Dept Nat & Math Sci, 8432 Magnolia Ave, Riverside, CA 92504 USA. RI Diemand, Juerg/G-9448-2011; Bullock, James/K-1928-2015; OI Bullock, James/0000-0003-4298-5082; Moustakas, Leonidas/0000-0003-3030-2360 FU NASA [NNX09AG01G]; National Aeronautics and Space Administration; Grainger Foundation; Swiss National Science Foundation (SNF); NASA ATP FX Halos 1 and 2 were run on the Cosmos computer cluster at JPL, and the Greenplanet computer cluster at UC Irvine. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. K.R.S. was partially supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. This research was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. A.B. acknowledges support from The Grainger Foundation. J.S.B. was partially supported by NASA grant NNX09AG01G. J.D. has been supported by the Swiss National Science Foundation (SNF). L.A.M. acknowledges NASA ATP support. NR 86 TC 50 Z9 50 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 MAY 20 PY 2013 VL 769 IS 1 AR 74 DI 10.1088/0004-637X/769/1/74 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500074 ER PT J AU Tal, T van Dokkum, PG Franx, M Leja, J Wake, DA Whitaker, KE AF Tal, Tomer van Dokkum, Pieter G. Franx, Marijn Leja, Joel Wake, David A. Whitaker, Katherine E. TI GALAXY ENVIRONMENTS OVER COSMIC TIME: THE NON- EVOLVING RADIAL GALAXY DISTRIBUTIONS AROUND MASSIVE GALAXIES SINCE z=1.6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: groups: general ID DIGITAL SKY SURVEY; SIMILAR-TO 3; LUMINOUS RED GALAXIES; MEDIUM-BAND SURVEY; INSIDE-OUT GROWTH; LENS ACS SURVEY; LESS-THAN 2; STELLAR MASS; STAR-FORMATION; DARK-MATTER AB We present a statistical study of the environments of massive galaxies in four redshift bins between z = 0.04 and z = 1.6, using data from the Sloan Digital Sky Survey and the NEWFIRM Medium Band Survey. We measure the projected radial distribution of galaxies in cylinders around a constant number density selected sample of massive galaxies and utilize a statistical subtraction of contaminating sources. Our analysis shows that massive primary galaxies typically live in group halos and are surrounded by 2-3 satellites with masses more than one-tenth of the primary galaxy mass. The cumulative stellar mass in these satellites roughly equals the mass of the primary galaxy itself. We further find that the radial number density profile of galaxies around massive primaries has not evolved significantly in either slope or overall normalization in the past 9.5 Gyr. A simplistic interpretation of this result can be taken as evidence for a lack of mergers in the studied groups and as support for a static evolution model of halos containing massive primaries. Alternatively, there exists a tight balance between mergers and accretion of new satellites such that the overall distribution of galaxies in and around the halo is preserved. The latter interpretation is supported by a comparison to a semi-analytic model, which shows a similar constant average satellite distribution over the same redshift range. C1 [Tal, Tomer] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [van Dokkum, Pieter G.; Leja, Joel] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Whitaker, Katherine E.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Tal, T (reprint author), Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. EM tal@ucolick.org OI Leja, Joel/0000-0001-6755-1315 FU NSF [AST-1202667, AST-0807974]; CT Space Grant; NASA [NNX11AB08G]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX T.T. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1202667.; We gratefully acknowledge support from the CT Space Grant, NSF grant AST-0807974, and NASA grant NNX11AB08G.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 85 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 31 DI 10.1088/0004-637X/769/1/31 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500031 ER PT J AU Townsend, RHD Rivinius, T Rowe, JF Moffat, AFJ Matthews, JM Bohlender, D Neiner, C Telting, JH Guenther, DB Kallinger, T Kuschnig, R Rucinski, SM Sasselov, D Weiss, WW AF Townsend, R. H. D. Rivinius, Th. Rowe, J. F. Moffat, A. F. J. Matthews, J. M. Bohlender, D. Neiner, C. Telting, J. H. Guenther, D. B. Kallinger, T. Kuschnig, R. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI MOST OBSERVATIONS OF sigma Ori E: CHALLENGING THE CENTRIFUGAL BREAKOUT NARRATIVE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: chemically peculiar; stars: early-type; stars: individual (HD 37479); stars: magnetic field; stars: rotation ID RIGIDLY ROTATING MAGNETOSPHERE; HELIUM-STRONG STARS; ORIONIS-E; MAGNETIC-FIELD; HR 7355-STAR; PHOTOMETRY; DISCOVERY; CLUSTER; SPACE; MODEL AB We present results from three weeks' photometric monitoring of the magnetic helium-strong star sigma Ori E using the Microvariability and Oscillations of Stars microsatellite. The star's light curve is dominated by twice-per-rotation eclipse-like dimmings arising when magnetospheric clouds transit across and occult the stellar disk. However, no evidence is found for any abrupt centrifugal breakout of plasma from the magnetosphere, either in the residual flux or in the depths of the light minima. Motivated by this finding we compare the observationally inferred magnetospheric mass against that predicted by a breakout analysis. The large discrepancy between the values leads us to argue that centrifugal breakout does not play a significant role in establishing the magnetospheric mass budget of sigma Ori E. C1 [Townsend, R. H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Rivinius, Th.] ESO European Org Astron Res Southern Hamisphere, Santiago 19001, Casilla, Chile. [Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Matthews, J. M.; Kallinger, T.; Kuschnig, R.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Bohlender, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Neiner, C.] Univ Paris Diderot, UPMC, Observatoire Paris, UMR 8109,CNRS,LESIA, F-92195 Meudon, France. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Kallinger, T.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Townsend, RHD (reprint author), Univ Wisconsin, Dept Astron, 2535 Sterling Hall,475 N Charter St, Madison, WI 53706 USA. EM townsend@astro.wisc.edu OI Kallinger, Thomas/0000-0003-3627-2561 FU NSF [AST-0908688, AST-0904607]; NASA [NNX12AC72G]; NSERC (Canada); Austrian Science Fund [P22691-N16] FX R.H.D.T. acknowledges support from NSF awards AST-0908688 and AST-0904607, and NASA award NNX12AC72G. A.F.J.M., D.B.G., J.M.M., and S.M.R. are grateful for financial support from NSERC (Canada). R.K. and W.W. acknowledge support by the Austrian Science Fund P22691-N16. NR 45 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 33 DI 10.1088/0004-637X/769/1/33 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500033 ER PT J AU Uritsky, VM Davila, JM Ofman, L Coyner, AJ AF Uritsky, Vadim M. Davila, Joseph M. Ofman, Leon Coyner, Aaron J. TI STOCHASTIC COUPLING OF SOLAR PHOTOSPHERE AND CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: photosphere; turbulence ID SELF-ORGANIZED CRITICALITY; EUV TRANSIENT BRIGHTENINGS; TURBULENT FINE-STRUCTURE; SPIRAL VORTEX MODEL; CURRENT-SHEET MODEL; MAGNETIC-FIELD; ACTIVE REGIONS; QUIET-SUN; ALFVEN WAVES; RESONANT ABSORPTION AB The observed solar activity is believed to be driven by the dissipation of nonpotential magnetic energy injected into the corona by dynamic processes in the photosphere. The enormous range of scales involved in the interaction makes it difficult to track down the photospheric origin of each coronal dissipation event, especially in the presence of complex magnetic topologies. In this paper, we propose an ensemble-based approach for testing the photosphere-corona coupling in a quiet solar region as represented by intermittent activity in Solar and Heliospheric Observatory Michelson Doppler Imager and Solar TErrestrial RElations Observatory Extreme Ultraviolet Imager image sets. For properly adjusted detection thresholds corresponding to the same degree of intermittency in the photosphere and corona, the dynamics of the two solar regions is described by the same occurrence probability distributions of energy release events but significantly different geometric properties. We derive a set of scaling relations reconciling the two groups of results and enabling statistical description of coronal dynamics based on photospheric observations. Our analysis suggests that multiscale intermittent dissipation in the corona at spatial scales >3 Mm is controlled by turbulent photospheric convection. Complex topology of the photospheric network makes this coupling essentially nonlocal and non-deterministic. Our results are in an agreement with the Parker's coupling scenario in which random photospheric shuffling generates marginally stable magnetic discontinuities at the coronal level, but they are also consistent with an impulsive wave heating involving multiscale Alfvenic wave packets and/or magnetohydrodynamic turbulent cascade. A back-reaction on the photosphere due to coronal magnetic reconfiguration can be a contributing factor. C1 [Uritsky, Vadim M.; Ofman, Leon] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Coyner, Aaron J.] Univ Tulsa, Tulsa, OK 74104 USA. RP Uritsky, VM (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM vadim.uritsky@nasa.gov FU NASA [NNG11PL10A 670.002, NNX12AB34G] FX We thank J. Klimchuk, S. Antiochos, M. Aschwanden, and M. Georgoulis for useful discussions and advice. The work of V.U. was supported by the NASA Grant NNG11PL10A 670.002 through the CUA's Institute for Astrophysics and Computational Sciences. L.O. was supported by NASA Grant NNX12AB34G. NR 147 TC 17 Z9 17 U1 2 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 62 DI 10.1088/0004-637X/769/1/62 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500062 ER PT J AU Wylezalek, D Galametz, A Stern, D Vernet, J De Breuck, C Seymour, N Brodwin, M Eisenhardt, PRM Gonzalez, AH Hatch, N Jarvis, M Rettura, A Stanford, SA Stevens, JA AF Wylezalek, Dominika Galametz, Audrey Stern, Daniel Vernet, Joel De Breuck, Carlos Seymour, Nick Brodwin, Mark Eisenhardt, Peter R. M. Gonzalez, Anthony H. Hatch, Nina Jarvis, Matt Rettura, Alessandro Stanford, Spencer A. Stevens, Jason A. TI GALAXY CLUSTERS AROUND RADIO-LOUD ACTIVE GALACTIC NUCLEI AT 1.3 < z < 3.2 AS SEEN BY SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: high-redshift; infrared: galaxies; techniques: photometric ID INFRARED ARRAY CAMERA; STELLAR POPULATION SYNTHESIS; H-ALPHA EMITTERS; SIMILAR-TO 2; HIGH-REDSHIFT; SPACE-TELESCOPE; X-RAY; MU-M; RED-SEQUENCE; SKY SURVEY AB Telescope snapshot program to investigate the environments of a large sample of obscured and unobscured luminous radio-loud active galactic nuclei (AGNs) at 1.2 < z < 3.2. These data, obtained for 387 fields, reach 3.6 and 4.5 mu m depths of [3.6] AB = 22.6 and [4.5] AB = 22.9 at the 95% completeness level, which is two to three times fainter than L* in this redshift range. By using the color cut [3.6] - [4.5] > -0.1 (AB), which efficiently selects high-redshift (z > 1.3) galaxies of all types, we identify galaxy cluster member candidates in the fields of the radio-loud AGN. The local density of these Infrared Array Camera (IRAC)-selected sources is compared to the density of similarly selected sources in blank fields. We find that 92% of the radio-loud AGN reside in environments richer than average. The majority (55%) of the radio-loud AGN fields are found to be overdense at a >= 2 sigma level; 10% are overdense at a >= 5 sigma level. A clear rise in surface density of IRAC-selected sources toward the position of the radio-loud AGN strongly supports an association of the majority of the IRAC-selected sources with the radio-loud AGN. Our results provide solid statistical evidence that radio-loud AGN are likely beacons for finding high-redshift galaxy (proto-) clusters. We investigate how environment depends on AGN type (unobscured radio-loud quasars versus obscured radio galaxies), radio luminosity and redshift, finding no correlation with either AGN type or radio luminosity. We find a decrease in density with redshift, consistent with galaxy evolution for this uniform, flux-limited survey. These results are consistent with expectations from the orientation-driven AGN unification model, at least for the high radio luminosity regimes considered in this sample. C1 [Wylezalek, Dominika; Stern, Daniel; Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wylezalek, Dominika; Vernet, Joel; De Breuck, Carlos] European So Observ, D-85748 Garching, Germany. [Galametz, Audrey] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Seymour, Nick] CASS, Epping, NSW 1710, Australia. [Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hatch, Nina] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Jarvis, Matt] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jarvis, Matt; Stevens, Jason A.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Jarvis, Matt] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Rettura, Alessandro] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, Spencer A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP Wylezalek, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Hatch, Nina/0000-0001-5600-0534; De Breuck, Carlos/0000-0002-6637-3315; Vernet, Joel/0000-0002-8639-8560; Seymour, Nicholas/0000-0003-3506-5536 FU ARC Future Fellowship; NASA FX We gratefully acknowledge James Falder and Conor Mancone who were involved in the initial CARLA proposals. N.S. is the recipient of an ARC Future Fellowship. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 74 TC 53 Z9 53 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR UNSP 79 DI 10.1088/0004-637X/769/1/79 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500079 ER PT J AU Kuang, S Newchurch, MJ Burris, J Liu, X AF Kuang, Shi Newchurch, Michael J. Burris, John Liu, Xiong TI Ground-based lidar for atmospheric boundary layer ozone measurements SO APPLIED OPTICS LA English DT Article ID ABSORPTION CROSS-SECTIONS; TROPOSPHERIC OZONE; VERTICAL-DISTRIBUTION; DIAL MEASUREMENTS; AEROSOL LIDAR; RAMAN LIDAR; TEMPERATURE; ULTRAVIOLET; ALGORITHM; PROFILES AB Ground-based lidars are suitable for long-term ozone monitoring as a complement to satellite and ozonesonde measurements. However, current ground-based lidars are unable to consistently measure ozone below 500 m above ground level (AGL) due to both engineering issues and high retrieval sensitivity to various measurement errors. In this paper, we present our instrument design, retrieval techniques, and preliminary results that focus on the high-temporal profiling of ozone within the atmospheric boundary layer (ABL) achieved by the addition of an inexpensive and compact mini-receiver to the previous system. For the first time, to the best of our knowledge, the lowest, consistently achievable observation height has been extended down to 125 m AGL for a ground-based ozone lidar system. Both the analysis and preliminary measurements demonstrate that this lidar measures ozone with a precision generally better than +/- 10% at a temporal resolution of 10 min and a vertical resolution from 150 m at the bottom of the ABL to 550 m at the top. A measurement example from summertime shows that inhomogeneous ozone aloft was affected by both surface emissions and the evolution of ABL structures. (C) 2013 Optical Society of America C1 [Kuang, Shi; Newchurch, Michael J.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. [Burris, John] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Kuang, S (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM kuang@nsstc.uah.edu RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X FU NASA's Science Mission Directorate; NOAA's National Environmental Satellite, Data, and Information Service (NESDIS) FX The authors thank Tom McGee of NASA/GSFC, Stuart McDermid, and Thierry Leblanc of NASA/JPL for extensive discussions about lidar instrumentation, Jack Kaye and Jay Al-Saadi of NASA/headquarters for continuing support, Wesley Cantrell and Guanyu Huang of UAHuntsville for providing the ozonesonde data, and Debra Hopson of the Huntsville Department of Natural Resources and Environmental Management for providing the surface ozone data. This work was supported by NASA's Science Mission Directorate and NOAA's National Environmental Satellite, Data, and Information Service (NESDIS). The UAHuntsville ozone lidar is affiliated with the Tropospheric Ozone Lidar NETwork (TOLNET) and the Network for Detection of Atmospheric Composition Change (NDACC). NR 53 TC 9 Z9 9 U1 1 U2 25 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X J9 APPL OPTICS JI Appl. Optics PD MAY 20 PY 2013 VL 52 IS 15 BP 3557 EP 3566 DI 10.1364/AO.52.003557 PG 10 WC Optics SC Optics GA 149SP UT WOS:000319341800014 PM 23736241 ER PT J AU Stephens, IW Looney, LW Kwon, W Hull, CLH Plambeck, RL Crutcher, RM Chapman, N Novak, G Davidson, J Vaillancourt, JE Shinnaga, H Matthews, T AF Stephens, Ian W. Looney, Leslie W. Kwon, Woojin Hull, Charles L. H. Plambeck, Richard L. Crutcher, Richard M. Chapman, Nicholas Novak, Giles Davidson, Jacqueline Vaillancourt, John E. Shinnaga, Hiroko Matthews, Tristan TI THE MAGNETIC FIELD MORPHOLOGY OF THE CLASS 0 PROTOSTAR L1157-mm SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: star formation; magnetic fields; polarization; stars: protostars ID 350 MU-M; STAR-FORMATION; SUBMILLIMETER POLARIZATION; MOLECULAR CLOUDS; IRAS 4A; CORES; OUTFLOW; DUST; POLARIMETRY; ENVELOPE AB We present the first detection of polarization around the Class 0 low-mass protostar L1157-mm at two different wavelengths. We show polarimetric maps at large scales (10 '' resolution at 350 mu m) from the SHARC-II Polarimeter and at smaller scales (1.'' 2-4.'' 5 at 1.3 mm) from the Combined Array for Research in Millimeter-wave Astronomy (CARMA). The observations are consistent with each other and show inferred magnetic field lines aligned with the outflow. The CARMA observations suggest a full hourglass magnetic field morphology centered about the core; this is only the second well-defined hourglass detected around a low-mass protostar to date. We apply two different methods to CARMA polarimetric observations to estimate the plane-of-sky magnetic field magnitude, finding values of 1.4 and 3.4 mG. C1 [Stephens, Ian W.; Looney, Leslie W.; Kwon, Woojin; Crutcher, Richard M.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Looney, Leslie W.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Kwon, Woojin] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Hull, Charles L. H.; Plambeck, Richard L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hull, Charles L. H.; Plambeck, Richard L.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Chapman, Nicholas; Novak, Giles; Matthews, Tristan] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Chapman, Nicholas; Novak, Giles; Matthews, Tristan] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Davidson, Jacqueline] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia. [Vaillancourt, John E.] NASA, SOFIA Sci Ctr, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA. [Shinnaga, Hiroko] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. RP Stephens, IW (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. EM stephen6@illinois.edu FU National Science Foundation [NSF AST 08-38226, AST-0838261]; CARMA partner universities; NSF [AST-090930] FX Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement (NSF AST 08-38226) and by the CARMA partner universities.; The Caltech Submillimeter Observatory is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261), and SHARP is supported by NSF grant AST-090930 to Northwestern University. NR 35 TC 20 Z9 20 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2013 VL 769 IS 1 AR L15 DI 10.1088/2041-8205/769/1/L15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151HN UT WOS:000319451400015 ER PT J AU Calabrese, E Hlozek, REA Battaglia, N Battistelli, ES Bond, JR Chluba, J Crichton, D Das, S Devlin, MJ Dunkley, J Dunner, R Farhang, M Gralla, MB Hajian, A Halpern, M Hasselfield, M Hincks, AD Irwin, KD Kosowsky, A Louis, T Marriage, TA Moodley, K Newburgh, L Niemack, MD Nolta, MR Page, LA Sehgal, N Sherwin, BD Sievers, JL Sifon, C Spergel, DN Staggs, ST Switzer, ER Wollack, EJ AF Calabrese, Erminia Hlozek, Renee E. A. Battaglia, Nick Battistelli, Elia S. Bond, J. Richard Chluba, Jens Crichton, Devin Das, Sudeep Devlin, Mark J. Dunkley, Joanna Duenner, Rolando Farhang, Marzieh Gralla, Megan B. Hajian, Amir Halpern, Mark Hasselfield, Matthew Hincks, Adam D. Irwin, Kent D. Kosowsky, Arthur Louis, Thibaut Marriage, Tobias A. Moodley, Kavilan Newburgh, Laura Niemack, Michael D. Nolta, Michael R. Page, Lyman A. Sehgal, Neelima Sherwin, Blake D. Sievers, Jonathan L. Sifon, Cristobal Spergel, David N. Staggs, Suzanne T. Switzer, Eric R. Wollack, Edward J. TI Cosmological parameters from pre-planck cosmic microwave background measurements SO PHYSICAL REVIEW D LA English DT Article ID CONSTRAINTS AB Recent data from the WMAP, ACT and SPT experiments provide precise measurements of the cosmic microwave background temperature power spectrum over a wide range of angular scales. The combination of these observations is well fit by the standard, spatially flat Lambda CDM cosmological model, constraining six free parameters to within a few percent. The scalar spectral index, n(s) = 0.9690 +/- 0.0089, is less than unity at the 3.5 sigma level, consistent with simple models of inflation. The damping tail of the power spectrum at high resolution, combined with the amplitude of gravitational lensing measured by ACT and SPT, constrains the effective number of relativistic species to be N-eff = 3.28 +/- 0.40, in agreement with the standard model's three species of light neutrinos. C1 [Calabrese, Erminia; Dunkley, Joanna; Louis, Thibaut] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Hlozek, Renee E. A.; Hasselfield, Matthew; Marriage, Tobias A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Battaglia, Nick] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Battistelli, Elia S.] Univ Rome Sapienza, Dept Phys, I-00185 Rome, Italy. [Bond, J. Richard; Farhang, Marzieh; Hajian, Amir; Hincks, Adam D.; Nolta, Michael R.; Switzer, Eric R.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Chluba, Jens; Crichton, Devin; Gralla, Megan B.; Marriage, Tobias A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Das, Sudeep] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Das, Sudeep] Univ Calif Berkeley, BCCP, LBL, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Devlin, Mark J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Duenner, Rolando] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Farhang, Marzieh] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Irwin, Kent D.; Niemack, Michael D.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Marriage, Tobias A.; Newburgh, Laura; Niemack, Michael D.; Page, Lyman A.; Sherwin, Blake D.; Sievers, Jonathan L.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Calabrese, E (reprint author), Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. RI Spergel, David/A-4410-2011; Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Chluba, Jens/0000-0003-3725-6096; Sievers, Jonathan/0000-0001-6903-5074; Sifon, Cristobal/0000-0002-8149-1352 FU U.S. National Science Foundation [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379]; Princeton University; Canada Foundation for Innovation (CFI); CFI under Compute Canada; Government of Ontario; University of Toronto; ERC [259505]; NASA Office of Space Science; University of Pennsylvania; Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); Ontario Research Fund-Research Excellence FX This work was supported by the U.S. National Science Foundation through Grants No. AST-0408698 and No. AST-0965625 for the ACT project, as well as Grants No. PHY-0855887 and No. PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund-Research Excellence; and the University of Toronto. Funding from ERC Grant No. 259505 supports E. C., J.D., and T. L. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. The likelihood code will be made public through LAMBDA [36] and the ACT website [37]. NR 31 TC 38 Z9 38 U1 1 U2 11 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 MAY 20 PY 2013 VL 87 IS 10 AR UNSP 103012 DI 10.1103/PhysRevD.87.103012 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 148OJ UT WOS:000319254500001 ER PT J AU de Viron, O Dickey, JO Ghil, M AF de Viron, O. Dickey, J. O. Ghil, M. TI Global modes of climate variability SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID NORTH-ATLANTIC OSCILLATION; SEA-SURFACE TEMPERATURES; OCEAN-ATMOSPHERE MODEL; INTERDECADAL VARIABILITY; HEMISPHERE WINTER; ENSO; REGIMES; FLOW AB The atmosphere, hydrosphere, and cryosphere form a fully coupled climate system. This system exhibits a number of large-scale phenomena, such as the El Nino-Southern Oscillation, the Asian Monsoon, the North Atlantic Oscillation, and the Madden-Julian Oscillation. While these modes of variability are not exactly periodic, they are oscillatory in character, and their state is monitored using so-called climate indices. Each of these scalar indices is a combination of several climate variables. Here we use a comprehensive set of 25 climate indices for time intervals that range between 1948 and 2011 and estimate an optimal set of lags between these indices to maximize their correlation. We show that most of the index pairs drawn from this set present a significant correlation on interannual time scales. It is also shown that on average, about two thirds of the total variability in each index can be described by using only the four leading principal components of the entire set of lagged indices. Our index set's leading orthogonal modes exhibit several interannual frequencies and capture separately variability associated with the North Atlantic and the North Pacific. These modes are associated, in turn, with large-scale variations of sea surface temperatures. C1 [de Viron, O.] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, UMR CNRS 7154, F-75013 Paris, France. [Dickey, J. O.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Ghil, M.] Ecole Normale Super, Dept Geosci, F-75231 Paris, France. [Ghil, M.] Ecole Normale Super, Lab Meteorol Dynam, CNRS, F-75231 Paris, France. [Ghil, M.] Ecole Normale Super, Lab Meteorol Dynam, IPSL, F-75231 Paris, France. [Ghil, M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Ghil, M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP de Viron, O (reprint author), Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, UMR CNRS 7154, F-75013 Paris, France. EM deviron@ipgp.fr RI de Viron, Olivier/N-6647-2014 OI de Viron, Olivier/0000-0003-3112-9686 FU U.S. National Science Foundation; Office of Naval Research; Institut Universitaire de France; Centre National des Etudes Spatiales through the TOSCA program; National Aeronautics and Space Administration (NASA) FX This study was supported by the U.S. National Science Foundation and the Office of Naval Research (MG), and by the Institut Universitaire de France and the Centre National des Etudes Spatiales through the TOSCA program (OdV). The work of JOD is a phase of research carried out at the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration (NASA). All but the MJO index time series were provided through the Earth System Research Laboratory web site at http://www.esrl.noaa.gov/psd/data/climateindices/list/. The MJO index time series comes from KNMI's Climate Explorer web site http://climexp.knmi.nl. It is a pleasure to thank the editor (Noah Diffenbaugh) and two anonymous reviewers for their help in improving the paper. NR 35 TC 12 Z9 13 U1 0 U2 21 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 MAY 16 PY 2013 VL 40 IS 9 BP 1832 EP 1837 DI 10.1002/grl.50386 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 163EC UT WOS:000320317500030 ER PT J AU Oikawa, E Nakajima, T Inoue, T Winker, D AF Oikawa, Eiji Nakajima, Teruyuki Inoue, Toshiro Winker, David TI A study of the shortwave direct aerosol forcing using ESSP/CALIPSO observation and GCM simulation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol direct effect; shortwave radiative forcing; CALIOP; SPRINTARS ID RESOLUTION IMAGING SPECTRORADIOMETER; CALIPSO LIDAR MEASUREMENTS; OPTICAL-PROPERTIES; SOLAR-RADIATION; CLOUD; MODEL; ABSORPTION; SCATTERING; SATELLITE; LAYERS AB Shortwave direct aerosol radiative forcing (DARF) is derived at the top of the atmosphere (TOA) and at the surface under clear-sky, cloudy-sky, and all-sky conditions using data of space-borne CALIOP lidar and MODIS sensor. We investigate four scenarios for evaluating the DARF: clear-sky, the case that aerosols exist above clouds, the case that aerosols exist below high-level clouds, and the case that aerosols are not detected by CALIOP in cloudy-sky condition. The cloudy-sky DARF is estimated by the latter three scenarios. The all-sky DARF is the combination of clear-sky and cloudy-sky DARF weighted by the cloud occurrence. They are then compared with DARF calculated by a global aerosol model, SPRINTARS. The results show that the TOA forcing over desert regions caused by dust with single scattering albedo (SSA) of 0.92 is positive regardless of cloud existence, due to high solar surface albedo. Off southern Africa, smoke aerosols with SSA of 0.84 above low-level clouds are observed and simulated and the annual mean TOA cloudy-sky DARF is estimated at more than +3 Wm-2, consistent with past studies. Aerosols with SSA of 0.96 within optically thin clouds cause a TOA negative forcing, while that within optically thick clouds cause a TOA positive forcing. This indicates that aerosols within optically thick clouds cause positive forcing in our radiative transfer calculation, regardless of SSA. Annual zonal averages of DARF from 60 degrees S to 60 degrees N under clear-sky, cloudy-sky, and all-sky are -2.97, +0.07, and -0.61 Wm-2 from CALIOP and -2.78, +1.07, and -0.58 Wm-2 from SPRINTARS. C1 [Oikawa, Eiji; Nakajima, Teruyuki; Inoue, Toshiro] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan. [Winker, David] NASA, Langley Res Ctr, Hampton, NH USA. RP Oikawa, E (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan. EM e_oikawa@aori.u-tokyo.ac.jp RI Nakajima, Teruyuki/H-2370-2013; INOUE, Toshiro/C-9597-2014 OI Nakajima, Teruyuki/0000-0002-9042-504X; FU MOE/GOSAT, MOE/GER [A1101] FX Part of this research was supported by funds from MOE/GOSAT, MOE/GER fund A1101, JST/CREST/EMS/TEEDDA, JAXA/EarthCARE and GCOM-C, MEXT/VL for climate diagnostics, MEXT/RECCA/SALSA, MEXT/KAKENHI/Innovative Areas 2409. We would like to thank D. Goto for providing the SPRINTARS simulation results and T. Nishizawa for discussing the SSA calculation and valuable comments. NR 50 TC 7 Z9 7 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 16 PY 2013 VL 118 IS 9 BP 3687 EP 3708 DI 10.1002/jgrd.50227 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 155JU UT WOS:000319744700018 ER PT J AU Doherty, RM Wild, O Shindell, DT Zeng, G MacKenzie, IA Collins, WJ Fiore, AM Stevenson, DS Dentener, FJ Schultz, MG Hess, P Derwent, RG Keating, TJ AF Doherty, R. M. Wild, O. Shindell, D. T. Zeng, G. MacKenzie, I. A. Collins, W. J. Fiore, A. M. Stevenson, D. S. Dentener, F. J. Schultz, M. G. Hess, P. Derwent, R. G. Keating, T. J. TI Impacts of climate change on surface ozone and intercontinental ozone pollution: A multi-model study SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE surface ozone; climate change; intercontinental transport; source-receptor relationships ID GLOBAL LIGHTNING DISTRIBUTIONS; AIR-QUALITY; ISOPRENE EMISSION; REACTIVE NITROGEN; CHEMISTRY MODEL; NORTH-AMERICA; UNITED-STATES; TRANSPORT; SENSITIVITY; PHOTOCHEMISTRY AB The impact of climate change between 2000 and 2095 SRES A2 climates on surface ozone (O)3 and on O3 source-receptor (S-R) relationships is quantified using three coupled climate-chemistry models (CCMs). The CCMs exhibit considerable variability in the spatial extent and location of surface O3 increases that occur within parts of high NOx emission source regions (up to 6 ppbv in the annual average and up to 14 ppbv in the season of maximum O3). In these source regions, all three CCMs show a positive relationship between surface O3 change and temperature change. Sensitivity simulations show that a combination of three individual chemical processes(i) enhanced PAN decomposition, (ii) higher water vapor concentrations, and (iii) enhanced isoprene emissionlargely reproduces the global spatial pattern of annual-mean surface O3 response due to climate change (R2=0.52). Changes in climate are found to exert a stronger control on the annual-mean surface O3 response through changes in climate-sensitive O3 chemistry than through changes in transport as evaluated from idealized CO-like tracer concentrations. All three CCMs exhibit a similar spatial pattern of annual-mean surface O3 change to 20% regional O3 precursor emission reductions under future climate compared to the same emission reductions applied under present-day climate. The surface O3 response to emission reductions is larger over the source region and smaller downwind in the future than under present-day conditions. All three CCMs show areas within Europe where regional emission reductions larger than 20% are required to compensate climate change impacts on annual-mean surface O3. C1 [Doherty, R. M.; MacKenzie, I. A.; Stevenson, D. S.] Univ Edinburgh, Sch GeoSci, Edinburgh EH8 9YL, Midlothian, Scotland. [Wild, O.] Univ Lancaster, Lancaster Environm Ctr, Lancaster, England. [Shindell, D. T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Shindell, D. T.] Columbia Univ, New York, NY USA. [Zeng, G.] Natl Inst Water & Atmospher Res, Lauder, New Zealand. [Collins, W. J.] Hadley Ctr, Met Off, Exeter, Devon, England. [Fiore, A. M.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Dentener, F. J.] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy. [Schultz, M. G.] Forschungszentrum Julich, Inst Energie & Klimaforsch Troposphare IEK 8, D-52425 Julich, Germany. [Hess, P.] Cornell Univ, Ithaca, NY USA. [Derwent, R. G.] Rdscientific, Newbury, Berks, England. [Keating, T. J.] US EPA, Off Policy Anal & Review, Washington, DC 20460 USA. [Collins, W. J.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Fiore, A. M.] Columbia Univ, Lamont Doherty Earth Observ, Dept Earth & Environm Sci, Palisades, NY USA. RP Doherty, RM (reprint author), Univ Edinburgh, Sch GeoSci, Edinburgh EH8 9YL, Midlothian, Scotland. EM ruth.doherty@ed.ac.uk RI Stevenson, David/C-8089-2012; Wild, Oliver/A-4909-2009; Collins, William/A-5895-2010; Shindell, Drew/D-4636-2012; Hess, Peter/M-3145-2015; Schultz, Martin/I-9512-2012 OI Derwent, Richard/0000-0003-4498-645X; Stevenson, David/0000-0002-4745-5673; Wild, Oliver/0000-0002-6227-7035; Collins, William/0000-0002-7419-0850; Hess, Peter/0000-0003-2439-3796; Schultz, Martin/0000-0003-3455-774X FU New Zealand Ministry of Science and Innovation; Office of Science and Technology through EPSRC's High End Computing Program FX We greatly thank Adam Butler for statistical expertise, advice, and insights. We are also extremely grateful to Owen Cooper for informal discussions and his review of the manuscript. We thank Paul Young and Larry Horowitz for insightful discussions. This work was performed under the Task Force on Hemispheric Transport of Air Pollution (www.htap.org). We thank the US EPA and European Commission for travel support to HTAP meetings. We also thank Michael Decker and Sabine Schroder for hosting the HTAP data repository at Forschungszentrum Juelich. GZ acknowledges NIWA HPCF facility and funding from New Zealand Ministry of Science and Innovation. RD and GZ thank Colin Johnson at the UK Met Office for provision of sea-surface temperature data, and RD thanks Lois Steenman-Clark and Grenville Lister for supercomputing support. This work made use of the facilities of HECToR, the UK's national high-performance computing service, which is provided by UoE HPCx Ltd at the University of Edinburgh, Cray Inc and NAG Ltd, and funded by the Office of Science and Technology through EPSRC's High End Computing Program. NR 66 TC 47 Z9 48 U1 3 U2 68 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 16 PY 2013 VL 118 IS 9 BP 3744 EP 3763 DI 10.1002/jgrd.50266 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 155JU UT WOS:000319744700022 ER PT J AU Jin, JJ Livesey, NJ Manney, GL Jiang, JH Schwartz, MJ Daffer, WH AF Jin, J. J. Livesey, N. J. Manney, G. L. Jiang, J. H. Schwartz, M. J. Daffer, W. H. TI Chemical discontinuity at the extratropical tropopause and isentropic stratosphere-troposphere exchange pathways diagnosed using Aura MLS data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Stratosphere-troposphere exchange; Tropopause; Microwave Limb Sounder; ozone; carbon monoxide ID POTENTIAL VORTICITY STREAMERS; ROSSBY-WAVE BREAKING; LOWERMOST STRATOSPHERE; NORTHERN-HEMISPHERE; MASS-EXCHANGE; EFFECTIVE DIFFUSIVITY; POLAR VORTEX; WATER-VAPOR; TRANSPORT; CLIMATOLOGY AB The chemical discontinuity at the extratropical tropopause (ExTP) and stratosphere-troposphere exchange (STE) pathways are investigated using the long-lived chemical species carbon monoxide (CO) and ozone (O3) measured by the Aura Microwave Limb Sounder (MLS). A relative coordinate, tropopause latitude (TpLat), is developed based on potential vorticity (PV) from the Goddard Earth Observing System version 5 (GEOS-5) data assimilation system. TpLat is defined as the shortest geographic distance along an isentropic surface from the extratropical tropopause (ExTP) to an observation location. Our results show that this coordinate highlights the sharp chemical discontinuities at the ExTP more clearly than the widely-used equivalent latitude coordinate. Geographical distributions of STE pathways and barriers are investigated based on meridional gradients in O3 abundances in the new TpLat coordinate in conjunction with analysis of Rossby wave breaking between 330 K and 360 K. In northern hemispheric (NH) winter (Dec-Jan-Feb), NH STE pathways are seen mainly above the northeast Pacific. In NH summer (Jun-Jul-Aug), the NH pathway covers all longitudes at 330 K. However, it is mainly located above Asia at 340 K and above the Atlantic and the North Pacific at 350 K and 360 K. In the southern hemisphere (SH), there is a weaker STE region above the Eastern Indian Ocean and the southwestern Pacific, at and above 350 K in SH winter, and a stronger STE region over the Southeastern Pacific at these levels during SH summer. In addition, this study shows NH PV gradients are slightly stronger near the ExTP in summer than in winter even though the subtropical jet is weaker and Rossby wave breaking is stronger in summer than in winter. C1 [Jin, J. J.; Livesey, N. J.; Manney, G. L.; Jiang, J. H.; Schwartz, M. J.; Daffer, W. H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Manney, G. L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. RP Jin, JJ (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD USA. EM jianjun.jin@nasa.gov RI Jin, Jianjun/G-8357-2012; Schwartz, Michael/F-5172-2016 OI Schwartz, Michael/0000-0001-6169-5094 NR 90 TC 1 Z9 1 U1 1 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 16 PY 2013 VL 118 IS 9 BP 3832 EP 3847 DI 10.1002/jgrd.50291 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 155JU UT WOS:000319744700028 ER PT J AU Saito, R Patra, PK Sweeney, C Machida, T Krol, M Houweling, S Bousquet, P Agusti-Panareda, A Belikov, D Bergmann, D Bian, HS Cameron-Smith, P Chipperfield, MP Fortems-Cheiney, A Fraser, A Gatti, LV Gloor, E Hess, P Kawa, SR Law, RM Locatelli, R Loh, Z Maksyutov, S Meng, L Miller, JB Palmer, PI Prinn, RG Rigby, M Wilson, C AF Saito, Ryu Patra, Prabir K. Sweeney, Colm Machida, Toshinobu Krol, Maarten Houweling, Sander Bousquet, Philippe Agusti-Panareda, Anna Belikov, Dmitry Bergmann, Dan Bian, Huisheng Cameron-Smith, Philip Chipperfield, Martyn P. Fortems-Cheiney, Audrey Fraser, Annemarie Gatti, Luciana V. Gloor, Emanuel Hess, Peter Kawa, Stephan R. Law, Rachel M. Locatelli, Robin Loh, Zoe Maksyutov, Shamil Meng, Lei Miller, John B. Palmer, Paul I. Prinn, Ronald G. Rigby, Matthew Wilson, Christopher TI TransCom model simulations of methane: Comparison of vertical profiles with aircraft measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE TransCom Methane; CH4 vertical profile; vertical; horizontal gradient ID CHEMICAL-TRANSPORT MODEL; ATMOSPHERIC CO2; TROPOSPHERE; STRATOSPHERE; VARIABILITY; SENSITIVITY; VERSION; OZONE; FLUX; AIR AB To assess horizontal and vertical transports of methane (CH4) concentrations at different heights within the troposphere, we analyzed simulations by 12 chemistry transport models (CTMs) that participated in the TransCom-CH4 intercomparison experiment. Model results are compared with aircraft measurements at 13 sites in Amazon/Brazil, Mongolia, Pacific Ocean, Siberia/Russia, and United States during the period of 2001-2007. The simulations generally show good agreement with observations for seasonal cycles and vertical gradients. The correlation coefficients of the daily averaged model and observed CH4 time series for the analyzed years are generally larger than 0.5, and the observed seasonal cycle amplitudes are simulated well at most sites, considering the between-model variances. However, larger deviations show up below 2 km for the model-observation differences in vertical profiles at some locations, e.g., at Santarem, Brazil, and in the upper troposphere, e.g., at Surgut, Russia. Vertical gradients and concentrations are underestimated at Southern Great Planes, United States, and Santarem and overestimated at Surgut. Systematic overestimation and underestimation of vertical gradients are mainly attributed to inaccurate emission and only partly to the transport uncertainties. However, large differences in model simulations are found over the regions/seasons of strong convection, which is poorly represented in the models. Overall, the zonal and latitudinal variations in CH4 are controlled by surface emissions below 2.5 km and transport patterns in the middle and upper troposphere. We show that the models with larger vertical gradients, coupled with slower horizontal transport, exhibit greater CH4 interhemispheric gradients in the lower troposphere. These findings have significant implications for the future development of more accurate CTMs with the possibility of reducing biases in estimated surface fluxes by inverse modeling. C1 [Saito, Ryu; Patra, Prabir K.] Res Inst Global Change JAMSTEC, Yokohama, Kanagawa 2360001, Japan. [Patra, Prabir K.] Tohoku Univ, Ctr Atmospher & Ocean Studies, Sendai, Miyagi 980, Japan. [Sweeney, Colm; Miller, John B.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Machida, Toshinobu; Belikov, Dmitry; Maksyutov, Shamil] Natl Inst Environm Studies, Ctr Global Environm Res, Tsukuba, Ibaraki, Japan. [Krol, Maarten] Univ Wageningen & Res Ctr, Wageningen, Netherlands. [Krol, Maarten; Houweling, Sander] SRON Netherlands Inst Space Res, Utrecht, Netherlands. [Bousquet, Philippe; Fortems-Cheiney, Audrey; Locatelli, Robin] Univ Versailles St Quentin Yvelines, Gif Sur Yvette, France. [Agusti-Panareda, Anna] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Bergmann, Dan; Cameron-Smith, Philip] Lawrence Livermore Natl Lab, Atmospher Earth & Energy Div, Livermore, CA USA. [Bian, Huisheng; Kawa, Stephan R.] NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. [Chipperfield, Martyn P.; Gloor, Emanuel; Wilson, Christopher] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds, W Yorkshire, England. [Fraser, Annemarie; Palmer, Paul I.] Univ Edinburgh, School GeoSci, Edinburgh, Midlothian, Scotland. [Gatti, Luciana V.] Inst Pesquisas Energet & Nucl, Div Quim Ambiental, Sao Paulo, Brazil. [Hess, Peter] Cornell Univ, Ithaca, NY USA. [Law, Rachel M.; Loh, Zoe] CSIRO Marine & Atmospher Res, Ctr Australian Weather & Climate Res, Aspendale, Vic, Australia. [Meng, Lei] Western Michigan Univ, Dept Geog, Kalamazoo, MI 49008 USA. [Meng, Lei] Western Michigan Univ, Environm Studies Program, Kalamazoo, MI 49008 USA. [Prinn, Ronald G.; Rigby, Matthew] MIT, Ctr Global Change Sci, Cambridge, MA 02139 USA. [Rigby, Matthew] Univ Bristol, Sch Chem, Bristol, Avon, England. RP Patra, PK (reprint author), Res Inst Global Change JAMSTEC, 3173-25 Showa Machi, Yokohama, Kanagawa 2360001, Japan. EM prabir@jamstec.go.jp RI Chipperfield, Martyn/H-6359-2013; Rigby, Matthew/A-5555-2012; Kawa, Stephan/E-9040-2012; Cameron-Smith, Philip/E-2468-2011; Law, Rachel/A-1969-2012; Meng, Lei/H-5253-2013; Fraser, Annemarie/D-3874-2012; Krol, Maarten/E-3414-2013; Bergmann, Daniel/F-9801-2011; Palmer, Paul/F-7008-2010; Maksyutov, Shamil/G-6494-2011; Hess, Peter/M-3145-2015; Belikov, Dmitry/I-9877-2016 OI Wilson, Chris/0000-0001-8494-0697; Chipperfield, Martyn/0000-0002-6803-4149; Rigby, Matthew/0000-0002-2020-9253; Cameron-Smith, Philip/0000-0002-8802-8627; Law, Rachel/0000-0002-7346-0927; Bergmann, Daniel/0000-0003-4357-6301; Maksyutov, Shamil/0000-0002-1200-9577; Hess, Peter/0000-0003-2439-3796; FU JSPS/MEXT KAKENHI-A [22241008]; UK Natural Environment Research Council National Centre for Earth Observation; NASA-AGAGE [NNX07AE89G, NNX11AF17G]; NERC Advanced Fellowship; NERC/NCEO; European Community [283576] FX This work was supported by JSPS/MEXT KAKENHI-A (grant 22241008). A. Fraser was supported by the UK Natural Environment Research Council National Centre for Earth Observation. We acknowledge the work of J. McGregor and M. Thatcher in the development of CCAM. CCAM simulations were undertaken as part of the Australian Climate Change Science Program and used the NCI National Facility in Canberra, ACT, Australia. R. Prinn andM. Rigby were supported by NASA-AGAGE grants NNX07AE89G and NNX11AF17G to MIT. M. Rigby was also supported by a NERC Advanced Fellowship. The TOMCAT work at the University of Leeds was supported by NERC/NCEO. The research leading to the IFS results has received funding from the European Community's Seventh Framework Programme [FP7 THEME (SPA.2011.1.5-02)] under grant 283576 in the context of the MACC-II project (Monitoring Atmospheric Composition and Climate-Interim Implementation). We sincerely thank all three anonymous reviewers for critical evaluation and providing very helpful comments and suggestions for improving the article. NR 36 TC 4 Z9 4 U1 0 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 16 PY 2013 VL 118 IS 9 BP 3891 EP 3904 DI 10.1002/jgrd.50380 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 155JU UT WOS:000319744700032 ER PT J AU Cuntz, M Quarles, B Eberle, J Shukayr, A AF Cuntz, M. Quarles, B. Eberle, J. Shukayr, A. TI On the Possibility of Habitable Moons in the System of HD 23079: Results from Orbital Stability Studies SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE astrobiology; instabilities; planetary systems; stars: individual: HD 23079; stars: late-type ID EXTRASOLAR PLANETARY SYSTEMS; CARBON-DIOXIDE CLOUDS; EARTH-LIKE PLANETS; EXOPLANETARY SYSTEMS; TROJAN PLANETS; GIANT PLANETS; NU OCTANTIS; IRREGULAR SATELLITES; TERRESTRIAL PLANETS; SUGGESTED PLANET AB The aim of our study is to investigate the possibility of habitable moons orbiting the giant planet HD 23079b, a Jupiter-mass planet, which follows a low-eccentricity orbit in the outer region of HD 23079's habitable zone. We show that HD 23079b is able to host habitable moons in prograde and retrograde orbits, as expected, noting that the outer stability limit for retrograde orbits is increased by nearly 90% compared with that of prograde orbits, a result consistent with previous generalised studies. For the targeted parameter space, it was found that the outer stability limit for habitable moons varies between 0.05236 and 0.06955 AU (prograde orbits) and between 0.1023 and 0.1190 AU (retrograde orbits), depending on the orbital parameters of the Jupiter-type planet if a minimum mass is assumed. These intervals correspond to 0.306 and 0.345 (prograde orbits) and 0.583 and 0.611 (retrograde orbits) of the planet's Hill radius. Larger stability limits are obtained if an increased value for the planetary mass m(p) is considered; they are consistent with the theoretically deduced relationship of m(p)(1/3). Finally, we compare our results with the statistical formulae of Domingos, Winter, & Yokoyama, indicating both concurrence and limitations. C1 [Cuntz, M.; Quarles, B.; Eberle, J.; Shukayr, A.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Quarles, B.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div 245 3, Moffett Field, CA 94035 USA. [Eberle, J.] North Lake Coll, Irving, TX 75038 USA. RP Cuntz, M (reprint author), Univ Texas Arlington, Dept Phys, POB 19059, Arlington, TX 76019 USA. EM cuntz@uta.edu FU SETI institute; U.S. Department of Education under GAANN [P200A090284]; University of Texas at Arlington FX This work has been supported by the SETI institute (M. C.), the U.S. Department of Education under GAANN grant no. P200A090284 (B. Q. and J.E.), and by the University of Texas at Arlington through its Research Enhancement Program (M. C. and A.S.). NR 67 TC 2 Z9 2 U1 0 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD MAY 15 PY 2013 VL 30 AR UNSP e033 DI 10.1017/pas.2013.011 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 168JY UT WOS:000320703000001 ER PT J AU Yee, HC Kotov, DV Wang, W Shu, CW AF Yee, H. C. Kotov, D. V. Wang, Wei Shu, Chi-Wang TI Spurious behavior of shock-capturing methods by the fractional step approach: Problems containing stiff source terms and discontinuities SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE High order numerical methods; Numerical combustion; Chemical reacting flows; Nonequilibrium flows; Stiff source terms; Numerical methods for stiff source terms with shocks; Wrong propagation speed of discontinuities ID NONLINEAR DIFFERENTIAL-EQUATIONS; HYPERBOLIC CONSERVATION-LAWS; STATE NUMERICAL-SOLUTIONS; REACTION-CONVECTION EQUATIONS; HIGH-ORDER METHODS; DIMENSIONAL DETONATIONS; SUBCELL RESOLUTION; DYNAMICAL-APPROACH; WAVE-PROPAGATION; EULER EQUATIONS AB The goal of this paper is to relate numerical dissipations that are inherited in high order shock-capturing schemes with the onset of wrong propagation speed of discontinuities. For pointwise evaluation of the source term, previous studies indicated that the phenomenon of wrong propagation speed of discontinuities is connected with the smearing of the discontinuity caused by the discretization of the advection term. The present study focuses only on solving the reactive system by the fractional step method using the Strang splitting. Studies shows that the degree of wrong propagation speed of discontinuities is highly dependent on the accuracy of the numerical method. The manner in which the smearing of discontinuities is contained by the numerical method and the overall amount of numerical dissipation being employed play major roles. Depending on the numerical method, time step and grid spacing, the numerical simulation may lead to (a) the correct solution (within the truncation error of the scheme), (b) a divergent solution, (c) a wrong propagation speed of discontinuities solution or (d) other spurious solutions that are solutions of the discretized counterparts but are not solutions of the governing equations. The findings might shed some light on the reported difficulties in numerical combustion and problems with stiff nonlinear (homogeneous) source terms and discontinuities in general. Published by Elsevier Inc. C1 [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kotov, D. V.] Stanford Ctr Turbulence Res, Stanford, CA 94305 USA. [Wang, Wei] Florida Int Univ, Dept Math & Stat, Miami, FL 33199 USA. [Shu, Chi-Wang] Brown Univ, Div Appl Math, Providence, RI 02912 USA. RP Yee, HC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Helen.M.Yee@nasa.gov FU DOE/SciDAC SAP grant [DE-AI02-06ER25796]; NASA; NASA [NNX12AJ62A] FX The support of the DOE/SciDAC SAP grant DE-AI02-06ER25796 and the collaboration with B. Sjogreen and A. Lani in developing the infrastructure of the nonequilibrium capability in the ADPDIS3D code used for this study are acknowledged. Insightful discussions throughout the course of this work with B. Sjogreen and NASA Ames colleagues M. Panesi, A. Wray and D. Prabhu are gratefully acknowledged. The work was performed by the second author as a postdoc fellow at the Center for Turbulence Research, Stanford University. The financial support from the NASA Fundamental Aeronautics (Hypersonic) Program for the first author is gratefully acknowledged. The research of C.-W. Shu and W. Wang is partially supported by NASA grant NNX12AJ62A. NR 56 TC 8 Z9 8 U1 0 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD MAY 15 PY 2013 VL 241 BP 266 EP 291 DI 10.1016/j.jcp.2013.01.028 PG 26 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 120QK UT WOS:000317186100015 ER PT J AU Huot, Y Franz, BA Fradette, M AF Huot, Yannick Franz, Bryan A. Fradette, Maxime TI Estimating variability in the quantum yield of Sun-induced chlorophyll fluorescence: A global analysis of oceanic waters SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Ocean color; Sun-induced fluorescence; Algorithm; Quantum yield ID COASTAL WATERS; REFLECTANCE SPECTRA; A FLUORESCENCE; CASE-1 WATERS; COLOR; PHYTOPLANKTON; ALGORITHMS; MODIS; SEA; SEAWIFS AB While empirical and semi-analytical algorithms that retrieve phytoplankton biomass from satellite ocean color have matured over the last few decades, the use of Sun-induced chlorophyll fluorescence data measured by spacebome sensors remains in its infancy. Sun-induced fluorescence has the potential to provide a synoptic global view of aspects of phytoplankton biology that go beyond biomass by observing the quantum yield of fluorescence. While several algorithms have been developed to retrieve the quantum yield, they are prone to biases from different sources. In this study, we assessed the accuracy of several ocean color algorithms to estimate phytoplankton chlorophyll or absorption when they are used together with Sun-induced fluorescence algorithms. Our analysis led us to develop a new type of algorithm for retrieving variability in the quantum yield of fluorescence. Based on a three dimensional lookup table, this algorithm avoided many of the biases present in older algorithms and provided distributions of the quantum yield that showed significant differences compared to previous methods. This algorithmic approach also has the advantage of being robust with respect to sensor characteristics and to the set of underlying proxies that are used, namely phytoplankton biomass, the absorption by chromophoric dissolved organic matter, and the incident irradiance. As such, it would be suitable for merging data from multiple satellite ocean color sensors. (C) 2013 Elsevier Inc. All rights reserved. C1 [Huot, Yannick] Univ Sherbrooke, Dept Geomat Appl, Ctr Applicat & Rech Teledetect, Sherbrooke, PQ J1K 2R1, Canada. [Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fradette, Maxime] Univ Sherbrooke, Dept Phys, Sherbrooke, PQ J1K 2R1, Canada. RP Huot, Y (reprint author), Univ Sherbrooke, Dept Geomat Appl, Ctr Applicat & Rech Teledetect, Sherbrooke, PQ J1K 2R1, Canada. EM yannickhuot@usherbrooke.ca; bryan.a.franz@nasa.gov; Maxime.Fradette@usherbrooke.ca RI Huot, Yannick/B-4497-2008; Franz, Bryan/D-6284-2012 OI Huot, Yannick/0000-0003-1793-761X; Franz, Bryan/0000-0003-0293-2082 NR 62 TC 10 Z9 10 U1 3 U2 65 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAY 15 PY 2013 VL 132 BP 238 EP 253 DI 10.1016/j.rse.2013.01.003 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 115SE UT WOS:000316831400020 ER PT J AU Sullivan, DF Dutta, SK Dreyer, M Gubrud, MA Roychowdhury, A Anderson, JR Lobb, CJ Wellstood, FC AF Sullivan, D. F. Dutta, S. K. Dreyer, M. Gubrud, M. A. Roychowdhury, A. Anderson, J. R. Lobb, C. J. Wellstood, F. C. TI Asymmetric superconducting quantum interference devices for suppression of phase diffusion in small Josephson junctions SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID CURRENT-VOLTAGE CHARACTERISTICS; TUNNEL-JUNCTIONS; COULOMB-BLOCKADE; ENVIRONMENT; NOISE AB We have measured the switching current versus applied magnetic flux of a highly asymmetric, hysteretic dc superconducting quantum interference device (SQUID) from 30 mK to 400 mK. The SQUID loop had an inductance of 1 nH, and the capacitances of the two Al-Al2O3-Al Josephson junctions comprising the SQUID were 100 fF and 5 fF. As expected, the switching current of the SQUID displayed a small, periodic modulation with applied flux, from which the switching currents of the large and small junctions at 30 mK were determined to be 846.3 +/- 0.1 nA and 0.7 +/- 0.08 nA, respectively. Measurements of an identically prepared small junction exhibited a highly suppressed switching current (I-S < 10 pA), consistent with phase diffusion in this device. The observed modulation in the SQUID thus demonstrates that the quantum mechanical uncertainty in the phase difference across the small junction was significantly reduced by coupling to the large junction through the loop inductance. We discuss the sensitivity of this technique for determining the gauge-invariant phase difference of small Josephson junctions, and the implications for imaging the phase of superconductors at the atomic scale using scanning tunneling microscopy. (C) 2013 AIP Publishing LLC. C1 [Sullivan, D. F.; Dutta, S. K.; Dreyer, M.; Gubrud, M. A.; Roychowdhury, A.; Anderson, J. R.; Lobb, C. J.; Wellstood, F. C.] Univ Maryland, Lab Phys Sci, College Pk, MD 20740 USA. [Sullivan, D. F.; Dutta, S. K.; Dreyer, M.; Gubrud, M. A.; Roychowdhury, A.; Anderson, J. R.; Lobb, C. J.; Wellstood, F. C.] Univ Maryland, Joint Quantum Inst, Dept Phys, College Pk, MD 20742 USA. [Sullivan, D. F.; Dutta, S. K.; Dreyer, M.; Gubrud, M. A.; Roychowdhury, A.; Anderson, J. R.; Lobb, C. J.; Wellstood, F. C.] Univ Maryland, Ctr Nanophys & Adv Mat, College Pk, MD 20742 USA. RP Sullivan, DF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM dan.f.sullivan@nasa.gov FU DOD; NSF FX We acknowledge many useful conversations with Dr. B. I. Barker, and financial support from the DOD and NSF. This work is dedicated to the fond memory of Dr. Kosta P. Vlahacos. NR 24 TC 3 Z9 3 U1 0 U2 10 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 MAY 14 PY 2013 VL 113 IS 18 AR 183905 DI 10.1063/1.4804057 PG 5 WC Physics, Applied SC Physics GA 149BX UT WOS:000319294100058 ER PT J AU Han, JW Kim, B Li, J Meyyappan, M AF Han, Jin-Woo Kim, Beomseok Li, Jing Meyyappan, M. TI A carbon nanotube based ammonia sensor on cotton textile SO APPLIED PHYSICS LETTERS LA English DT Article ID SMART TEXTILE; ELECTRODES; FABRICS AB A single-wall carbon nanotube (CNT) based ammonia (NH3) sensor was implemented on a cotton yarn. Two types of sensors were fabricated: Au/sensing CNT/Au and conducting/sensing/conducting all CNT structures. Two perpendicular Au wires were designed to contact CNT-cotton yarn for metal-CNT sensor, whereas nanotubes were used for the electrode as well as sensing material for the all CNT sensor. The resistance shift of the CNT network upon NH3 was monitored in a chemiresistor approach. The CNT-cotton yarn sensors exhibited uniformity and repeatability. Furthermore, the sensors displayed good mechanical robustness against bending. The present approach can be utilized for low-cost smart textile applications. C1 [Han, Jin-Woo; Kim, Beomseok; Li, Jing; Meyyappan, M.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Han, JW (reprint author), NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov NR 23 TC 18 Z9 18 U1 8 U2 48 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 MAY 13 PY 2013 VL 102 IS 19 AR 193104 DI 10.1063/1.4805025 PG 4 WC Physics, Applied SC Physics GA 164WB UT WOS:000320440800083 ER PT J AU Mignolet, MP Przekop, A Rizzi, SA Spottswood, SM AF Mignolet, Marc P. Przekop, Adam Rizzi, Stephen A. Spottswood, S. Michael TI A review of indirect/non-intrusive reduced order modeling of nonlinear geometric structures SO JOURNAL OF SOUND AND VIBRATION LA English DT Review ID SMOOTH ORTHOGONAL DECOMPOSITION; YAWED SUPERSONIC-FLOW; PANEL FLUTTER; SYSTEM-IDENTIFICATION; AEROELASTIC MODES; RESPONSE ANALYSIS; FREE-VIBRATIONS; BASIS SELECTION; ACTIVE CONTROL; PLATES AB The paper presents a review of reduced order modeling (ROM) techniques for geometrically nonlinear structures, more specifically of those techniques that are applicable to structural models constructed using commercial finite element software. The form of the ROM governing equations, the estimation of their parameters, and the selection of the basis functions are reviewed in detail and comparisons of predicted displacements and stresses obtained by the ROM and the full order, finite element models are presented. These ROM methods and validations are extended next to multidisciplinary problems in which the structure is subjected to thermal effects or interacts with the aerodynamics/ acoustics. These various applications demonstrate the usefulness and appropriateness of ROMs as computationally efficient alternatives to full finite element models for the accurate prediction of the geometrically nonlinear response of the structures considered. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Mignolet, Marc P.] Arizona State Univ, SEMTE, Fac Mech Engn, Tempe, AZ 85287 USA. [Mignolet, Marc P.] Arizona State Univ, SEMTE, Fac Aerosp Engn, Tempe, AZ 85287 USA. [Przekop, Adam] Analyt Mech Associates Inc, Hampton, VA 23666 USA. [Rizzi, Stephen A.] NASA, Struct Acoust Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Spottswood, S. Michael] USAF, AFRL RQSS Struct Sci Ctr, Res Lab, Wright Patterson AFB, OH 45433 USA. RP Mignolet, MP (reprint author), Arizona State Univ, SEMTE, Fac Mech Engn, Tempe, AZ 85287 USA. EM marc.mignolet@asu.edu NR 81 TC 33 Z9 33 U1 4 U2 49 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X EI 1095-8568 J9 J SOUND VIB JI J. Sound Vibr. PD MAY 13 PY 2013 VL 332 IS 10 BP 2437 EP 2460 DI 10.1016/j.jsv.2012.10.017 PG 24 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 113CA UT WOS:000316642600005 ER PT J AU Lorenzo, CF Hartley, TT Malti, R AF Lorenzo, C. F. Hartley, T. T. Malti, R. TI Application of the principal fractional meta-trigonometric functions for the solution of linear commensurate-order time-invariant fractional differential equations SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE fractional differential equations; fractional meta-trigonometric functions; R-function AB A new and simplified method for the solution of linear constant coefficient fractional differential equations of any commensurate order is presented. The solutions are based on the R-function and on specialized Laplace transform pairs derived from the principal fractional meta-trigonometric functions. The new method simplifies the solution of such fractional differential equations and presents the solutions in the form of real functions as opposed to fractional complex exponential functions, and thus is directly applicable to real-world physics. C1 [Lorenzo, C. F.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Hartley, T. T.] Univ Akron, Dept Elect & Comp Engn, Akron, OH 44325 USA. [Malti, R.] Univ Bordeaux, IMS UMR CNRS 5218, F-33405 Talence, France. RP Lorenzo, CF (reprint author), NASA Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM carl.f.lorenzo@nasa.gov FU NASA Glenn Research Center FX The authors gratefully acknowledge the support of the NASA Glenn Research Center. NR 18 TC 2 Z9 2 U1 0 U2 3 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD MAY 13 PY 2013 VL 371 IS 1990 SI SI AR 20120151 DI 10.1098/rsta.2012.0151 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 117GS UT WOS:000316942100007 PM 23547228 ER PT J AU Ramsey, BD Atkins, C Gubarev, MV Kilaru, K O'Dell, SL AF Ramsey, B. D. Atkins, C. Gubarev, M. V. Kilaru, K. O'Dell, S. L. TI Optics requirements for x-ray astronomy and developments at the Marshall Space Flight Center SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 4th International Workshop on Metrology for X-ray Optics, Mirror Design and Fabrication CY JUL 04-06, 2012 CL Barcelona, SPAIN DE X-ray optics; X-ray astronomy; Replicated; Active control ID HIGH-RESOLUTION AB X-ray optics have revolutionized x-ray astronomy; the degree of background suppression that these afford has led to a tremendous increase in sensitivity. The current Chandra observatory has the same collecting area (similar to 10(3) cm(2)) as that of the non-imaging UHURU observatory, the first x-ray observatory which was launched in 1970, but has five orders of magnitude more sensitivity due to its focusing optics. In addition, its 0.5 '' angular resolution has revealed a wealth of structure in many cosmic x-ray sources. The Chandra observatory achieved its resolution by using relatively thick pieces of Zerodur glass, which were meticulously figured and polished to form the four-shell nested array. The resulting optical assembly weighed > 1000 kg, and cost approximately $0.5B. The challenge for future x-ray astronomy missions is to greatly increase the collecting area (by one or more orders of magnitude) while ultimately maintaining sub-arcsecond angular resolution, and all within realistic mass and budget constraints. Published by Elsevier B.V. C1 [Ramsey, B. D.; Gubarev, M. V.; Kilaru, K.; O'Dell, S. L.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35805 USA. [Atkins, C.] Univ Alabama, Dept Phys, Huntsville, AL 35805 USA. RP Ramsey, BD (reprint author), NASA, George C Marshall Space Flight Ctr, Astrophys Off, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM Brian.Ramsey@nasa.gov OI O'Dell, Stephen/0000-0002-1868-8056 NR 17 TC 4 Z9 4 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD MAY 11 PY 2013 VL 710 BP 143 EP 150 DI 10.1016/j.nima.2012.10.119 PG 8 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 133HD UT WOS:000318128600027 ER PT J AU Abedin, MN Bradley, AT Ismail, S Sharma, SK Sandford, SP AF Abedin, M. Nurul Bradley, Arthur T. Ismail, Syed Sharma, Shiv K. Sandford, Stephen P. TI Compact remote multisensing instrument for planetary surfaces and atmospheres characterization SO APPLIED OPTICS LA English DT Article ID RAMAN-SPECTROSCOPY; SPECTRA; METERS; MARS; MINERALS; SYSTEM AB This paper describes a prototype feasibility demonstration system of a multipurpose Raman-fluorescence spectrograph and compact lidar system suitable for planetary sciences missions. The key measurement features of this instrument are its abilities to: i) detect minerals and organics at low levels in the dust constituents of surface, subsurface material and rocks on Mars, ii) determine the distribution of trace fluorescent ions with time-resolved fluorescence spectroscopy to learn about the geological conditions under which these minerals formed, iii) inspect material toxicity from a mobile robotic platform during local site characterization, iv) measure dust aerosol and cloud distributions, v) measure near-field atmospheric carbon dioxide, and vi) identify surface CO2-ice, surface water ice, and surface or subsurface methane hydrate. This prototype instrument and an improved follow-on design are described and have the capability for scientific investigations discussed above, to remotely investigate geological processes from a robotic platformat more than a 20-m radial distance with potential to go beyond 100 m. It also provides single wavelength (532 nm) aerosol/cloud profiling over very long ranges (>10 km with potential to 20 km). Measurement results obtained with this prototype unit from a robotic platform and calculated potential performance are presented in this paper. (c) 2013 Optical Society of America C1 [Abedin, M. Nurul] NASA, Langley Res Ctr, Remote Sensing Flight Syst Branch, Hampton, VA 23681 USA. [Bradley, Arthur T.] NASA, Langley Res Ctr, Elect Syst Branch, Hampton, VA 23681 USA. [Ismail, Syed] NASA, Langley Res Ctr, Atmospher Chem & Dynam Branch, Hampton, VA 23681 USA. [Sharma, Shiv K.] Univ Hawaii, Hawaii Inst Geophys & Planetol HIGH, Honolulu, HI 96822 USA. [Sandford, Stephen P.] NASA, Langley Res Ctr, Space Technol & Explorat Directorate, Hampton, VA 23681 USA. RP Abedin, MN (reprint author), NASA, Langley Res Ctr, Remote Sensing Flight Syst Branch, 5 N Dryden St,MS 468, Hampton, VA 23681 USA. EM m.n.abedin@nasa.gov FU NASA Mars Instrument Development Project through NASA LaRC; University of Hawaii FX The authors would like to thanks to Mr. Joshua Hibberd, Mr. Chris Garcia, Mr. Johnny Mau, Dr. Tamer Refaat, Mr. Ben Robinson, Mr. George Lockard, Mr. Nathaneal Miller, Mr. Terry Mack, Mr. Frank Boyer, and Mr. Kevin Mitchell for their constant hard work to bring this prototype instrument into a success. In addition, we acknowledge NASA Langley Research Center for constant support on remote Raman, fluorescence, and lidar activities from robotic platform through NASA Langley's investment funds. This program has been supported in part by a joint NASA Mars Instrument Development Project through NASA LaRC and University of Hawaii. NR 34 TC 3 Z9 3 U1 0 U2 17 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X J9 APPL OPTICS JI Appl. Optics PD MAY 10 PY 2013 VL 52 IS 14 BP 3116 EP 3126 DI 10.1364/AO.52.003116 PG 11 WC Optics SC Optics GA 145DP UT WOS:000318994500001 ER PT J AU Huang, XC Fortenberry, RC Lee, TJ AF Huang, Xinchuan Fortenberry, Ryan C. Lee, Timothy J. TI SPECTROSCOPIC CONSTANTS AND VIBRATIONAL FREQUENCIES FOR l-C3H+ AND ISOTOPOLOGUES FROM HIGHLY ACCURATE QUARTIC FORCE FIELDS: THE DETECTION OF l-C3H+ IN THE HORSEHEAD NEBULA PDR QUESTIONED SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: individual objects (Horsehead nebula); ISM: lines and bands; ISM: molecules; molecular data; radio lines: ISM ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; AB-INITIO; LINEAR C3H3+; ENERGY; CHEMISTRY; CATIONS; HCNH+ AB Very recently, molecular rotational transitions observed in the photon-dominated region of the Horsehead nebula have been attributed to l-C3H+. In an effort to corroborate this finding, we employed state-of-the-art and proven high-accuracy quantum chemical techniques to compute spectroscopic constants for this cation and its isotopologues. Even though the B rotational constant from the fit of the observed spectrum and our computations agree to within 20 MHz, a typical level of accuracy, the D rotational constant differs by more than 40%, while the H rotational constant differs by three orders of magnitude. With the likely errors in the rotational transition energies resulting from this difference in D on the order of 1 MHz for the lowest observed transition (J = 4 -> 3) and growing as J increases, the assignment of the observed rotational lines from the Horsehead nebula to l-C3H+ is questionable. C1 [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Huang, XC (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA. EM Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013 FU NASA/SETI Institute [NNX12AG96A]; NASA; NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant [NNH10ZDA001N] FX X.H. received funding from the NASA/SETI Institute Cooperative Agreements NNX12AG96A. The NASA Postdoctoral Program administered by Oak Ridge Associated Universities funded R.C.F. Support from NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant (NNH10ZDA001N) is gratefully acknowledged. The CheMVP program was used to create Figure 1. Additionally, the authors thank Dr. Michael C. McCarthy of the Harvard-Smithsonian Center for Astrophysics and Dr. David W. Schwenke of NASA Ames Research Center for useful discussions and explorations related to this project. NR 48 TC 14 Z9 14 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 10 PY 2013 VL 768 IS 2 AR L25 DI 10.1088/2041-8205/768/2/L25 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FN UT WOS:000318347700002 ER PT J AU Russell, DM Russell, TD Miller-Jones, JCA O'Brien, K Soria, R Sivakoff, GR Slaven-Blair, T Lewis, F Markoff, S Homan, J Altamirano, D Curran, PA Rupen, MP Belloni, TM Bel, MC Casella, P Corbel, S Dhawan, V Fender, RP Gallo, E Gandhi, P Heinz, S Kording, EG Krimm, HA Maitra, D Migliari, S Remillard, RA Sarazin, CL Shahbaz, T Tudose, V AF Russell, D. M. Russell, T. D. Miller-Jones, J. C. A. O'Brien, K. Soria, R. Sivakoff, G. R. Slaven-Blair, T. Lewis, F. Markoff, S. Homan, J. Altamirano, D. Curran, P. A. Rupen, M. P. Belloni, T. M. Cadolle Bel, M. Casella, P. Corbel, S. Dhawan, V. Fender, R. P. Gallo, E. Gandhi, P. Heinz, S. Kording, E. G. Krimm, H. A. Maitra, D. Migliari, S. Remillard, R. A. Sarazin, C. L. Shahbaz, T. Tudose, V. TI AN EVOLVING COMPACT JET IN THE BLACK HOLE X-RAY BINARY MAXI J1836-194 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; ISM: jets and outflows; X-rays: binaries ID GX 339-4; MULTIWAVELENGTH OBSERVATIONS; DISK-WIND; OUTBURST; CANDIDATE; EMISSION; STATES; SPECTRUM; DISTRIBUTIONS; TRANSITIONS AB We report striking changes in the broadband spectrum of the compact jet of the black hole transient MAXI J1836-194 over state transitions during its discovery outburst in 2011. A fading of the optical-infrared (IR) flux occurred as the source entered the hard-intermediate state, followed by a brightening as it returned to the hard state. The optical-IR spectrum was consistent with a power law from optically thin synchrotron emission, except when the X-ray spectrum was softest. By fitting the radio to optical spectra with a broken power law, we constrain the frequency and flux of the optically thick/thin break in the jet synchrotron spectrum. The break gradually shifted to higher frequencies as the source hardened at X-ray energies, from similar to 10(11) to similar to 4 x 10(13) Hz. The radiative jet luminosity integrated over the spectrum appeared to be greatest when the source entered the hard state during the outburst decay (although this is dependent on the high-energy cooling break, which is not seen directly), even though the radio flux was fading at the time. The physical process responsible for suppressing and reactivating the jet (neither of which are instantaneous but occur on timescales of weeks) is uncertain, but could arise from the varying inner accretion disk radius regulating the fraction of accreting matter that is channeled into the jet. This provides an unprecedented insight into the connection between inflow and outflow, and has implications for the conditions required for jets to be produced, and hence their launching process. C1 [Russell, D. M.; Shahbaz, T.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Russell, D. M.; Shahbaz, T.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Russell, T. D.; Miller-Jones, J. C. A.; Soria, R.; Slaven-Blair, T.; Curran, P. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [O'Brien, K.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Sivakoff, G. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Lewis, F.] Univ Glamorgan, Faulkes Telescope Project, Pontypridd CF37 1DL, M Glam, Wales. [Lewis, F.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Markoff, S.; Altamirano, D.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Homan, J.; Remillard, R. A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rupen, M. P.; Dhawan, V.] NRAO Domenici Sci Operat Ctr, Socorro, NM 87801 USA. [Belloni, T. M.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Cadolle Bel, M.] European Space Agcy, European Space Astron Ctr, ISOC, Madrid, Spain. [Casella, P.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Corbel, S.] Univ Paris Diderot, CNRS, CEA DSM, IRFU SAp,Lab AIM,UMR 7158, Gif Sur Yvette, France. [Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Gallo, E.; Maitra, D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Gandhi, P.] Japan Aerosp Explorat Agcy, ISAS, Chuo Ku, Sagamihara, Kanagawa 2298510, Japan. [Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Heinz, S.] Univ Wisconsin Madison, Dept Astron, Madison, WI 53706 USA. [Kording, E. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] USRA, Columbia, MD 21044 USA. [Migliari, S.] Univ Barcelona IEEC UB, ICC, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Tudose, V.] Inst Space Sci, RO-077125 Bucharest, Romania. RP Russell, DM (reprint author), Inst Astrofis Canarias, E-38200 Tenerife, Spain. EM russell@iac.es RI Curran, Peter/B-5293-2013; Sivakoff, Gregory/G-9602-2011; Miller-Jones, James/B-2411-2013; Tudose, Valeriu/F-8976-2010; OI Russell, Thomas/0000-0001-6958-8891; Casella, Piergiorgio/0000-0002-0752-3301; Curran, Peter/0000-0003-3003-4626; Sivakoff, Gregory/0000-0001-6682-916X; Miller-Jones, James/0000-0003-3124-2814; Heinz, Sebastian/0000-0002-8433-8652 FU ESO Program [087.D-0914, 089.D-0970]; European Community [IEF 274805]; Australian Research Council [DP120102393]; FP7 grant [ITN 215212 Black Hole Universe]; Spanish Ministry of Economy and Competitiveness (MINECO) project [AYA2010-18080]; ANR "CHAOS" [ANR-12-BS05-0009]; Smithsonian Institution; Academia Sinica FX Based on observations collected at the European Southern Observatory, Chile, under ESO Program IDs 087.D-0914 and 089.D-0970.; D.M.R. thanks Mario van den Ancker and Christian Hummel at ESO for help with the preparation and execution of the VLT/VISIR observations. D. M. R. acknowledges support from a Marie Curie Intra European Fellowship within the 7th European Community Framework Programme (FP7) under contract No. IEF 274805. This work was supported by Australian Research Council grant DP120102393, FP7 grant agreement No. ITN 215212 Black Hole Universe, the Spanish Ministry of Economy and Competitiveness (MINECO) project AYA2010-18080, and ANR "CHAOS" (ANR-12-BS05-0009). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica. The Faulkes Telescope South is maintained and operated by Las Cumbres Observatory Global Telescope Network. NR 49 TC 26 Z9 26 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 10 PY 2013 VL 768 IS 2 AR L35 DI 10.1088/2041-8205/768/2/L35 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FN UT WOS:000318347700012 ER PT J AU Barclay, T Burke, CJ Howell, SB Rowe, JF Huber, D Isaacson, H Jenkins, JM Kolbl, R Marcy, GW Quintana, EV Still, M Twicken, JD Bryson, ST Borucki, WJ Caldwell, DA Ciardi, D Clarke, BD Christiansen, JL Coughlin, JL Fischer, DA Li, J Haas, MR Hunter, R Lissauer, JJ Mullally, F Sabale, A Seader, SE Smith, JC Tenenbaum, P Uddin, AKMK Thompson, SE AF Barclay, Thomas Burke, Christopher J. Howell, Steve B. Rowe, Jason F. Huber, Daniel Isaacson, Howard Jenkins, Jon M. Kolbl, Rea Marcy, Geoffrey W. Quintana, Elisa V. Still, Martin Twicken, Joseph D. Bryson, Stephen T. Borucki, William J. Caldwell, Douglas A. Ciardi, David Clarke, Bruce D. Christiansen, Jessie L. Coughlin, Jeffrey L. Fischer, Debra A. Li, Jie Haas, Michael R. Hunter, Roger Lissauer, Jack J. Mullally, Fergal Sabale, Anima Seader, Shawn E. Smith, Jeffrey C. Tenenbaum, Peter Uddin, A. K. M. Kamal Thompson, Susan E. TI A SUPER-EARTH-SIZED PLANET ORBITING IN OR NEAR THE HABITABLE ZONE AROUND A SUN-LIKE STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: fundamental parameters; stars: individual (Kepler-69, KIC 8692861, KOI-172); stars: statistics; techniques: photometric ID STELLAR EVOLUTION DATABASE; SOLAR-TYPE STARS; ERROR-CORRECTION; LIGHT CURVES; MILKY-WAY; KEPLER; CANDIDATES; EXOPLANET; SCIENCE; MULTIPLICITY AB We present the discovery of a super-Earth-sized planet in or near the habitable zone of a Sun-like star. The host is Kepler-69, a 13.7 mag G4V-type star. We detect two periodic sets of transit signals in the 3-year flux time series of Kepler-69, obtained with the Kepler spacecraft. Using the very high precision Kepler photometry, and follow-up observations, our confidence that these signals represent planetary transits is >99.3%. The inner planet, Kepler-69b, has a radius of 2.24(-0.29)(+0.44) R-circle plus and orbits the host star every 13.7 days. The outer planet, Kepler-69c, is a super-Earth-sized object with a radius of 1.7(-0.23)(+0.34) R-circle plus and an orbital period of 242.5 days. Assuming an Earth-like Bond albedo, Kepler-69c has an equilibrium temperature of 299 +/- 19 K, which places the planet close to the habitable zone around the host star. This is the smallest planet found by Kepler to be orbiting in or near the habitable zone of a Sun-like star and represents an important step on the path to finding the first true Earth analog. C1 [Barclay, Thomas; Burke, Christopher J.; Howell, Steve B.; Rowe, Jason F.; Huber, Daniel; Jenkins, Jon M.; Quintana, Elisa V.; Still, Martin; Twicken, Joseph D.; Bryson, Stephen T.; Borucki, William J.; Caldwell, Douglas A.; Clarke, Bruce D.; Christiansen, Jessie L.; Coughlin, Jeffrey L.; Li, Jie; Haas, Michael R.; Hunter, Roger; Lissauer, Jack J.; Mullally, Fergal; Seader, Shawn E.; Smith, Jeffrey C.; Tenenbaum, Peter; Thompson, Susan E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Burke, Christopher J.; Rowe, Jason F.; Jenkins, Jon M.; Quintana, Elisa V.; Twicken, Joseph D.; Caldwell, Douglas A.; Clarke, Bruce D.; Christiansen, Jessie L.; Coughlin, Jeffrey L.; Li, Jie; Mullally, Fergal; Seader, Shawn E.; Smith, Jeffrey C.; Tenenbaum, Peter; Thompson, Susan E.] SETI Inst, Mountain View, CA 94043 USA. [Isaacson, Howard; Kolbl, Rea; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Ciardi, David] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Sabale, Anima; Uddin, A. K. M. Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Barclay, T (reprint author), NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi, David/0000-0002-5741-3047 FU NASA Science Mission Directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission Directorate. Some Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. We used data from the UKIRT Wide Field Camera (WFCAM; Casali et al. 2007) and a photometric system described in Hewett et al. (2006). The pipeline processing and science archive are described in Hambly et al. (2008). D.H. is supported by appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 59 TC 27 Z9 27 U1 2 U2 26 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 MAY 10 PY 2013 VL 768 IS 2 AR 101 DI 10.1088/0004-637X/768/2/101 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400004 ER PT J AU Ellingson, SW Clarke, TE Craig, J Hicks, BC Lazio, TJW Taylor, GB Wilson, TL Wolfe, CN AF Ellingson, S. W. Clarke, T. E. Craig, J. Hicks, B. C. Lazio, T. J. W. Taylor, G. B. Wilson, T. L. Wolfe, C. N. TI OBSERVATIONS OF CRAB GIANT PULSES IN 20-84 MHz USING LWA1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Crab Nebula); ISM: structure; pulsars: general; pulsars: individual (Crab Pulsar); scattering ID NEBULA PULSAR; RADIO SOURCES; SCATTERING; DISPERSION; VARIABILITY; BURSTS; SYSTEM; ARRAY; CAS AB We report the detection and observed characteristics of giant pulses from the Crab Nebula pulsar (B0531+21) in four frequency bands covering 20-84 MHz using the recently completed Long Wavelength Array Station 1 (LWA1) radio telescope. In 10 hr of observations distributed over a 72 day period in fall of 2012, 33 giant pulses having peak flux densities between 400 Jy and 2000 Jy were detected. Twenty-two of these pulses were detected simultaneously in channels of 16 MHz bandwidth centered at 44 MHz, 60 MHz, and 76 MHz, including one pulse which was also detected in a channel centered at 28 MHz. We quantify statistics of pulse amplitude and pulse shape characteristics, including pulse broadening. Amplitude statistics are consistent with expectations based on extrapolations from previous work at higher and lower frequencies. Pulse broadening is found to be relatively high, but not significantly greater than expected. We present procedures that have been found to be effective for observing giant pulses in this frequency range. C1 [Ellingson, S. W.; Wolfe, C. N.] Virginia Tech, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24060 USA. [Clarke, T. E.; Hicks, B. C.; Wilson, T. L.] USN, Res Lab, Washington, DC 20375 USA. [Craig, J.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ellingson, SW (reprint author), Virginia Tech, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24060 USA. FU 6.1 base funding; Office of Naval Research [N00014-07-C-0147]; National Science Foundation of the University Radio Observatories program [AST-1139963, AST-1139974]; National Radio Astronomy Observatory FX The authors acknowledge helpful discussions with W. A. Coles, T. H. Hankins, J. F. Helmboldt, N. E. Kassim, W. A. Majid, and B. J. Rickett. Some of the data presented in this paper were processed using the LWA1 User Computing Facility, which is a joint project of the University of New Mexico, Virginia Tech, and the Jet Propulsion Laboratory and in which J. Dowell was the primary contributor. Basic research in astronomy at the Naval Research Laboratory is supported by 6.1 base funding. Construction of LWA1 was supported by the Office of Naval Research under Contract N00014-07-C-0147. Support for operations and continuing development of LWA1 is provided by the National Science Foundation under grants AST-1139963 and AST-1139974 of the University Radio Observatories program. The authors acknowledge the support of the National Radio Astronomy Observatory. NR 34 TC 8 Z9 8 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 136 DI 10.1088/0004-637X/768/2/136 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400039 ER PT J AU Garcia, J Dauser, T Reynolds, CS Kallman, TR McClintock, JE Wilms, J Eikmann, W AF Garcia, J. Dauser, T. Reynolds, C. S. Kallman, T. R. McClintock, J. E. Wilms, J. Eikmann, W. TI X-RAY REFLECTED SPECTRA FROM ACCRETION DISK MODELS. III. A COMPLETE GRID OF IONIZED REFLECTION CALCULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; atomic processes; black hole physics; line: formation; radiative transfer; X-rays: general ID ACTIVE GALACTIC NUCLEI; K-SHELL PHOTOIONIZATION; RESONANT AUGER DESTRUCTION; PLANE-PARALLEL GEOMETRY; FINITE-DENSITY PLASMAS; BLACK-HOLE SYSTEMS; ATOMIC DECAY DATA; COLD MATTER; IRON LINES; DIELECTRONIC RECOMBINATION AB We present a new and complete library of synthetic spectra for modeling the component of emission that is reflected from an illuminated accretion disk. The spectra were computed using an updated version of our code XILLVER that incorporates new routines and a richer atomic database. We offer in the form of a table model an extensive grid of reflection models that cover a wide range of parameters. Each individual model is characterized by the photon index G of the illuminating radiation, the ionization parameter xi at the surface of the disk (i.e., the ratio of the X-ray flux to the gas density), and the iron abundance A(Fe) relative to the solar value. The ranges of the parameters covered are 1.2 <= Gamma <= 3.4, 1 <= xi <= 10(4), and 0.5 <= A(Fe) <= 10. These ranges capture the physical conditions typically inferred from observations of active galactic nuclei, and also stellar-mass black holes in the hard state. This library is intended for use when the thermal disk flux is faint compared to the incident power-law flux. The models are expected to provide an accurate description of the Fe K emission line, which is the crucial spectral feature used to measure black hole spin. A total of 720 reflection spectra are provided in a single FITS file (http://hea-www.cfa.harvard.edu/similar to javier/xillver/) suitable for the analysis of X-ray observations via the atable model in XSPEC. Detailed comparisons with previous reflection models illustrate the improvements incorporated in this version of XILLVER. C1 [Garcia, J.; McClintock, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Garcia, J.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Dauser, T.; Wilms, J.; Eikmann, W.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.; Wilms, J.; Eikmann, W.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Reynolds, C. S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Garcia, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; thomas.dauser@sternwarte.uni-erlangen.de; chris@astro.umd.edu; timothy.r.kallman@nasa.gov; jem@cfa.harvard.edu; joern.wilms@sternwarte.uni-erlangen.de; wiebke.eikmann@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 NR 96 TC 82 Z9 82 U1 1 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 MAY 10 PY 2013 VL 768 IS 2 AR 146 DI 10.1088/0004-637X/768/2/146 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400049 ER PT J AU Guillemot, L Kramer, M Johnson, TJ Craig, HA Romani, RW Venter, C Harding, AK Ferdman, RD Stairs, IH Kerr, M AF Guillemot, L. Kramer, M. Johnson, T. J. Craig, H. A. Romani, R. W. Venter, C. Harding, A. K. Ferdman, R. D. Stairs, I. H. Kerr, M. TI FERMI LAT PULSED DETECTION OF PSR J0737-3039A IN THE DOUBLE PULSAR SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; pulsars: general; pulsars: individual (PSR J0737-3039A, PSR J0737-3039B) ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; RELATIVISTIC SPIN PRECESSION; LIGHT CURVES; MILLISECOND PULSARS; EMISSION GEOMETRY; RADIO; POLARIZATION; RADIATION; MODEL AB We report the Fermi Large Area Telescope discovery of gamma-ray pulsations from the 22.7 ms pulsar A in the double pulsar system J0737-3039A/B. This is the first mildly recycled millisecond pulsar (MSP) detected in the GeV domain. The 2.7 s companion object PSR J0737-3039B is not detected in gamma rays. PSR J0737-3039A is a faint gamma-ray emitter, so that its spectral properties are only weakly constrained; however, its measured efficiency is typical of other MSPs. The two peaks of the gamma-ray light curve are separated by roughly half a rotation and are well offset from the radio and X-ray emission, suggesting that the GeV radiation originates in a distinct part of the magnetosphere from the other types of emission. From the modeling of the radio and the gamma-ray emission profiles and the analysis of radio polarization data, we constrain the magnetic inclination a and the viewing angle zeta to be close to 90 degrees, which is consistent with independent studies of the radio emission from PSR J0737-3039A. A small misalignment angle between the pulsar's spin axis and the system's orbital axis is therefore favored, supporting the hypothesis that pulsar B was formed in a nearly symmetric supernova explosion as has been discussed in the literature already. C1 [Guillemot, L.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kramer, M.; Ferdman, R. D.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Johnson, T. J.] Natl Acad Sci, Washington, DC 20001 USA. [Craig, H. A.; Romani, R. W.; Kerr, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Craig, H. A.; Romani, R. W.; Kerr, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ferdman, R. D.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Stairs, I. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Guillemot, L (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM guillemo@mpifr-bonn.mpg.de RI Venter, Christo/E-6884-2011 OI Venter, Christo/0000-0002-2666-4812 FU Commonwealth of Australia FX We are very grateful to Richard N. Manchester (ATNF) for providing valuable comments which helped to improve the manuscript, for providing us with the Parkes polarization data analyzed in this paper, and for carrying out independent cross-checks of the relative alignment of the radio and gamma-ray profiles using Parkes timing data taken concurrently with the Fermi dataset. The Parkes radio telescope is part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by the Commonwealth Scientific and Industrial Research Organisation (CSIRO). NR 46 TC 11 Z9 11 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 MAY 10 PY 2013 VL 768 IS 2 AR 169 DI 10.1088/0004-637X/768/2/169 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400072 ER PT J AU Hjorth, J Vreeswijk, PM Gall, C Watson, D AF Hjorth, Jens Vreeswijk, Paul M. Gall, Christa Watson, Darach TI ON INFERRING EXTINCTION LAWS IN z similar to 6 QUASARS AS SIGNATURES OF SUPERNOVA DUST SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; dust, extinction; galaxies: high-redshift; quasars: general ID DIGITAL SKY SURVEY; INTERSTELLAR-MEDIUM; EARLY UNIVERSE; HIGH-REDSHIFT; SDSSP J104433.04-012502.2; Z-SIMILAR-TO-6 QUASARS; SPECTRAL PROPERTIES; INFRARED-SPECTRA; ACCRETION DISKS; II SUPERNOVAE AB Unusual extinction curves of high-redshift QSOs have been taken as evidence that dust is primarily produced by supernovae at high redshift. In particular, the 3000 angstrom Todini-Ferrara-Maiolino kink in the extinction curve of the z = 6.20 SDSS J1048+4637 has been attributed to supernova dust. Here we discuss the challenges in inferring robust extinction curves of high-redshift QSOs and critically assess previous claims of detection of supernova dust. In particular, we address the sensitivity to the choice of intrinsic QSO spectrum, the need for a long wavelength baseline, and the drawbacks in fitting theoretical extinction curves. In a sample of 21 QSOs at z similar to 6 we detect significant ultraviolet extinction using existing broadband optical, near-infrared, and Spitzer photometry. The median extinction curve is consistent with a Small Magellanic Cloud curve with A(1450) similar to 0.7 mag and does not exhibit any conspicuous (rest frame) 2175 angstrom or 3000 angstrom features. For two QSOs, SDSS J1044-0125 at z = 5.78 and SDSS J1030+0524 at z = 6.31, we further present X-shooter spectra covering the wavelength range 0.9-2.5 mu m. The resulting non-parametric extinction curves do not exhibit the 3000 angstrom kink. Finally, in a re-analysis of literature spectra of SDSS J1048+4637, we do not find evidence for a conspicuous kink. We conclude that the existing evidence for a 3000 angstrom feature is weak and that the overall dust properties at high and low redshifts show no significant differences. This, however, does not preclude supernovae from dominating the dust budget at high redshift. C1 [Hjorth, Jens; Vreeswijk, Paul M.; Gall, Christa; Watson, Darach] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Vreeswijk, Paul M.] Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Vreeswijk, Paul M.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Gall, Christa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hjorth, J (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM jens@dark-cosmology.dk; paul.vreeswijk@weizmann.ac.il; christa.gall@nasa.gov; darach@dark-cosmology.dk RI Hjorth, Jens/M-5787-2014; Watson, Darach/E-4521-2015; Gall, Christa/P-7630-2016 OI Hjorth, Jens/0000-0002-4571-2306; Watson, Darach/0000-0002-4465-8264; Gall, Christa/0000-0002-8526-3963 FU European Southern Observatory, Paranal, Chile (ESO) [084.D-0360(A)]; NASA Postdoctoral Program (NPP); Danish National Research Foundation FX Based on observations collected at the European Southern Observatory, Paranal, Chile (ESO programme ID 084.D-0360(A)).; We thank Linhua Jiang and Marianne Vestergaard for providing tables of the broadband photometry and the black-hole masses (from Jiang et al. 2010) used in this paper and Martin Pessah for helpful discussions. We thank Simona Gallerani, Hiroyuki Hirashita, Roberto Maiolino, Dan Perley, and an anonymous referee for comments on the manuscript. C. G. is supported from the NASA Postdoctoral Program (NPP). The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 81 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 173 DI 10.1088/0004-637X/768/2/173 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400076 ER PT J AU Hull, CLH Plambeck, RL Bolatto, AD Bower, GC Carpenter, JM Crutcher, RM Fiege, JD Franzmann, E Hakobian, NS Heiles, C Houde, M Hughes, AM Jameson, K Kwon, W Lamb, JW Looney, LW Matthews, BC Mundy, L Pillai, T Pound, MW Stephens, IW Tobin, JJ Vaillancourt, JE Volgenau, NH Wright, MCH AF Hull, Charles L. H. Plambeck, Richard L. Bolatto, Alberto D. Bower, Geoffrey C. Carpenter, John M. Crutcher, Richard M. Fiege, Jason D. Franzmann, Erica Hakobian, Nicholas S. Heiles, Carl Houde, Martin Hughes, A. Meredith Jameson, Katherine Kwon, Woojin Lamb, James W. Looney, Leslie W. Matthews, Brenda C. Mundy, Lee Pillai, Thushara Pound, Marc W. Stephens, Ian W. Tobin, John J. Vaillancourt, John E. Volgenau, N. H. Wright, Melvyn C. H. TI MISALIGNMENT OF MAGNETIC FIELDS AND OUTFLOWS IN PROTOSTELLAR CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: magnetic fields; magnetic fields; polarization; stars: formation; stars: magnetic field; stars: protostars ID STAR-FORMING REGIONS; VLBA DETERMINATION; DUST POLARIZATION; MOLECULAR CLOUD; DISK FORMATION; H2O MASERS; T-TAURI; DISTANCE; ORION; MILLIMETER AB We present results of lambda 1.3 mm dust-polarization observations toward 16 nearby, low-mass protostars, mapped with similar to 2 ''.5 resolution at CARMA. The results show that magnetic fields in protostellar cores on scales of similar to 1000 AU are not tightly aligned with outflows from the protostars. Rather, the data are consistent with scenarios where outflows and magnetic fields are preferentially misaligned (perpendicular), or where they are randomly aligned. If one assumes that outflows emerge along the rotation axes of circumstellar disks, and that the outflows have not disrupted the fields in the surrounding material, then our results imply that the disks are not aligned with the fields in the cores from which they formed. C1 [Hull, Charles L. H.; Plambeck, Richard L.; Bower, Geoffrey C.; Heiles, Carl; Hughes, A. Meredith; Wright, Melvyn C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hull, Charles L. H.; Plambeck, Richard L.; Bower, Geoffrey C.; Heiles, Carl; Hughes, A. Meredith; Wright, Melvyn C. H.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Bolatto, Alberto D.; Jameson, Katherine; Mundy, Lee; Pound, Marc W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bolatto, Alberto D.; Jameson, Katherine; Mundy, Lee; Pound, Marc W.] Univ Maryland, Lab Millimeter Wave Astron, College Pk, MD 20742 USA. [Carpenter, John M.; Lamb, James W.; Pillai, Thushara] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Crutcher, Richard M.; Hakobian, Nicholas S.; Kwon, Woojin; Looney, Leslie W.; Stephens, Ian W.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Fiege, Jason D.; Franzmann, Erica] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Houde, Martin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Kwon, Woojin] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Looney, Leslie W.; Tobin, John J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Matthews, Brenda C.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Matthews, Brenda C.] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Vaillancourt, John E.] NASA, Ames Res Ctr, Univ Space Res Assoc, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Volgenau, N. H.] Owens Valley Radio Observ, Big Pine, CA 93513 USA. RP Hull, CLH (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM chat@astro.berkeley.edu FU NSF Graduate Fellowship; NSERC Discovery grant; NASA through Hubble Fellowship [HST-HF-51300.01-A]; Space Telescope Science Institute; NASA [NAS 5-26555]; CAREER grant [NSF-AST0955836, NSF-AST1139998]; Research Corporation for Science Advancement Cottrell Scholar award; state of California; state of Illinois; state of Maryland; James S. McDonnell Foundation; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; University of Chicago; Associates of the California Institute of Technology; National Science Foundation; CARMA partner universities FX C.L.H.H. acknowledges support from an NSF Graduate Fellowship. J.D.F. acknowledges support from an NSERC Discovery grant. J.J.T. acknowledges support provided by NASA through Hubble Fellowship grant #HST-HF-51300.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. A.D.B. acknowledges support from a CAREER grant NSF-AST0955836, NSF-AST1139998, and a Research Corporation for Science Advancement Cottrell Scholar award.; Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. NR 43 TC 54 Z9 54 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 159 DI 10.1088/0004-637X/768/2/159 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400062 ER PT J AU Randol, BM McComas, DJ Schwadron, NA AF Randol, B. M. McComas, D. J. Schwadron, N. A. TI INTERSTELLAR PICK-UP IONS OBSERVED BETWEEN 11 AND 22 AU BY NEW HORIZONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: atoms; solar wind; Sun: heliosphere ID PITCH-ANGLE SCATTERING; WIND TERMINATION SHOCK; SOLAR-WIND; TURBULENCE TRANSPORT; DISTRIBUTIONS; HELIOSPHERE; VELOCITY; HYDROGEN; PROTONS; PLASMA AB We report new observations by the Solar Wind Around Pluto instrument on the New Horizons spacecraft, which measures energy per charge (E/q) spectra of solar wind and interstellar pick-up ions (PUIs) between 11 AU and 22 AU from the Sun. The data provide an unprecedented look at PUIs as there have been very few measurements of PUIs beyond 10 AU. We analyzed the PUI part of the spectra by comparing them to the classic Vasyliunas and Siscoe PUI model. Our analysis indicates that PUIs are usually well-described by this distribution. We derive parameters relevant to PUI studies, such as the ionization rate normalized to 1 AU. Our result for the average ionization rate between 11 and 12 AU agrees with an independently derived average value found during the same time. Later, we find a general increase in the ionization rate, which is consistent with the increase in solar activity. We also calculate the PUI thermal pressure, which appears to be roughly consistent with previous results. Through fitting of the solar wind proton peaks in our spectra, we derive solar wind thermal pressures. Based on our analysis, we predict a ratio of PUI thermal pressure to solar wind thermal pressure just inside the termination shock to be between 100 and >1000. C1 [Randol, B. M.; McComas, D. J.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA. [Randol, B. M.; McComas, D. J.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX USA. [Schwadron, N. A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Randol, BM (reprint author), Goddard Space Flight Ctr, Code 672, Greenbelt, MD USA. EM brentrandol@gmail.com FU SWAP instrument work on the NASA New Horizons mission [NASW-02008] FX We thank all the members of the SWAP and New Horizons teams without whom this work would not have been possible. This work was funded as a part of the SWAP instrument work on the NASA New Horizons mission (Contract No. NASW-02008). NR 35 TC 6 Z9 6 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 120 DI 10.1088/0004-637X/768/2/120 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400023 ER PT J AU Sayers, J Czakon, NG Mantz, A Golwala, SR Ameglio, S Downes, TP Koch, PM Lin, KY Maughan, BJ Molnar, SM Moustakas, L Mroczkowski, T Pierpaoli, E Shitanishi, JA Siegel, S Umetsu, K Van der Pyl, N AF Sayers, J. Czakon, N. G. Mantz, A. Golwala, S. R. Ameglio, S. Downes, T. P. Koch, P. M. Lin, K. -Y. Maughan, B. J. Molnar, S. M. Moustakas, L. Mroczkowski, T. Pierpaoli, E. Shitanishi, J. A. Siegel, S. Umetsu, K. Van der Pyl, N. TI SUNYAEV-ZEL'DOVICH-MEASURED PRESSURE PROFILES FROM THE BOLOCAM X-RAY/SZ GALAXY CLUSTER SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium ID MASS-TEMPERATURE RELATION; SOUTH-POLE TELESCOPE; INTRACLUSTER MEDIUM; REPRESENTATIVE SAMPLE; SECONDARY CALIBRATORS; SCALING RELATIONS; OUTER REGIONS; BETA-MODEL; XMM-NEWTON; HOT GAS AB We describe Sunyaev-Zel'dovich (SZ) effect measurements and analysis of the intracluster medium (ICM) pressure profiles of a set of 45 massive galaxy clusters imaged using Bolocam at the Caltech Submillimeter Observatory. We deproject the average pressure profile of our sample into 13 logarithmically spaced radial bins between 0.07R(500) and 3.5R(500), and we find that a generalized Navarro, Frenk, and White (gNFW) profile describes our data with sufficient goodness-of-fit and best-fit parameters (C-500, alpha, beta, gamma, P-0 = 1.18, 0.86, 3.67, 0.67, 4.29). We use X-ray data to define cool-core and disturbed subsamples of clusters, and we constrain the average pressure profiles of each of these subsamples. We find that, given the precision of our data, the average pressure profiles of disturbed and cool-core clusters are consistent with one another at R greater than or similar to 0.15R(500), with cool-core systems showing indications of higher pressure at R less than or similar to 0.15R500. In addition, for the first time, we place simultaneous constraints on the mass scaling of cluster pressure profiles, their ensemble mean profile, and their radius-dependent intrinsic scatter between 0.1R(500) and 2.0R(500). The scatter among profiles is minimized at radii between similar or equal to 0.2R(500) and similar or equal to 0.5R(500), with a value of similar or equal to 20%. These results for the intrinsic scatter are largely consistent with previous analyses, most of which have relied heavily on X-ray derived pressures of clusters at significantly lower masses and redshifts compared to our sample. Therefore, our data provide further evidence that cluster pressure profiles are largely universal with scatter of similar or equal to 20%-40% about the universal profile over a wide range of masses and redshifts. C1 [Sayers, J.; Czakon, N. G.; Golwala, S. R.; Downes, T. P.; Mroczkowski, T.; Siegel, S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Mantz, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ameglio, S.; Pierpaoli, E.; Shitanishi, J. A.] Univ So Calif, Los Angeles, CA 90089 USA. [Koch, P. M.; Lin, K. -Y.; Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Maughan, B. J.; Van der Pyl, N.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Molnar, S. M.] Natl Taiwan Univ, LeCosPA Ctr, Taipei 10617, Taiwan. [Moustakas, L.; Mroczkowski, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sayers, J (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. EM jack@caltech.edu OI Mroczkowski, Tony/0000-0003-3816-5372; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360; Pierpaoli, Elena/0000-0002-7957-8993 FU NASA; NASA through the Einstein Fellowship Program [PF0-110077]; NASA Graduate Student Research Fellowship; National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; Academia Sinica Career Development Award; National Aeronautics and Space Administration; [NSF/AST-0838261]; [NASA/NNX11AB07G]; [NSF/AST-0838187]; [NASA/NNX07AH59G] FX We acknowledge the assistance of the following: the day crew and Hilo staff of the Caltech Submillimeter Observatory, who provided invaluable assistance during data-taking for this data set; Kathy Deniston, Barbara Wertz, and Diana Bisel, who provided effective administrative support at Caltech and in Hilo; Matt Hollister and Matt Ferry, who assisted in the collection of these data; and the referee, who provided numerous useful suggestions. The Bolocam observations were supported by the Gordon and Betty Moore Foundation. J.S. was supported by a NASA Graduate Student Research Fellowship, a NASA Post-doctoral Program Fellowship, NSF/AST-0838261 and NASA/NNX11AB07G; T. M. was supported by NASA through the Einstein Fellowship Program grant PF0-110077; N.C. was partially supported by a NASA Graduate Student Research Fellowship; A. M. was partially supported by NSF/AST-0838187; S. A., E. P., and J.A.S. were partially supported by NASA/NNX07AH59G; K. U. acknowledges partial support from the National Science Council of Taiwan grant NSC100-2112-M-001-008-MY3 and from the Academia Sinica Career Development Award. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research made use of the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (NSF/AST-0838261). NR 79 TC 43 Z9 43 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 MAY 10 PY 2013 VL 768 IS 2 AR 177 DI 10.1088/0004-637X/768/2/177 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400080 ER PT J AU Yoonessi, M Scheiman, DA Dittler, M Peck, JA Ilavsky, J Gaier, JR Meador, MA AF Yoonessi, Mitra Scheiman, Daniel A. Dittler, Matthew Peck, John A. Ilavsky, Jan Gaier, James R. Meador, Michael A. TI High-temperature multifunctional rnagnetoactive nickel graphene polyimide nanocomposites SO POLYMER LA English DT Article DE Polymer nanocomposites; Hybrid nanoparticles; Polymer actuators ID SHAPE-MEMORY; FUNCTIONALIZED GRAPHENE; LAYER GRAPHENE; OXIDE; NANOPARTICLES; ACTUATORS; COMPOSITE; GRAPHITE; SCATTERING; FILMS AB Composite Nickel graphene nanoparticles with hybrid magnetic and electrical properties were prepared. Nickel nanoparticles were tethered to the graphene through a carbon layers and were covered with an amorphous carbon layer to protect them from oxidation. Ni-graphene polyimide nanocomposites were prepared and exhibited magnetic characteristics and high electrical conductivity. The saturation magnetization of the polyimide nanocomposites increased with increasing magnetic nanoparticle content. First order reversal curve (FORC) magnetization showed a bimodal size distribution of the magnetic nanoparticles. Ultra-small-angle X-ray scattering (USAXS) of the nickel nanoparticles in Ni-graphene polyimide nanocomposites were estimated by a sphere model with bimodal size distribution. Nickel graphene nanoparticles were examined by high-resolution transmission electron microscopy (HR-TEM) where two size ranges of nickel were observed. Ni-graphene nanoparticles were well dispersed in the polyimide resin when examined by HR-TEM. Ni-graphene polyimide nanocomposites exhibited magnetic actuation when exposed to a static magnetic field. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Yoonessi, Mitra] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Scheiman, Daniel A.] ASRC, Cleveland, OH 44135 USA. [Dittler, Matthew; Gaier, James R.; Meador, Michael A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Peck, John A.] Univ Akron, Dept Polymer Engn, Akron, OH 44325 USA. [Ilavsky, Jan] Argonne Natl Lab, Argonne, IL 60439 USA. RP Yoonessi, M (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. EM mitra.yoonessi@gmail.com RI USAXS, APS/D-4198-2013 FU Subsonics Fixed Wing Project, Fundamental Aeronautics Program under NASA [NNC07BA13B]; National Science Foundation/Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357] FX This research was funded by the Subsonics Fixed Wing Project, Fundamental Aeronautics Program under NASA Contract NNC07BA13B. We appreciate the support of Dave Hull, Anna Palczer of NASA-GRC for the TEM and high temperature TGA. Richard Rogers is thanked for his wide angle X-ray scattering support. We express our appreciation to the Advanced Photon Source, Argonne National Laboratory, for providing the access to the USAXS beamline. ChemMatCARS Sector 15 is principally supported by National Science Foundation/Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-06CH11357. The NASA-GRC USRP program, Dave Kankam, is greatly appreciated for the student support. NR 56 TC 10 Z9 11 U1 7 U2 118 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0032-3861 EI 1873-2291 J9 POLYMER JI Polymer PD MAY 9 PY 2013 VL 54 IS 11 BP 2776 EP 2784 DI 10.1016/j.polymer.2013.03.015 PG 9 WC Polymer Science SC Polymer Science GA 141TB UT WOS:000318748300021 ER PT J AU Kharecha, PA Hansen, JE AF Kharecha, Pushker A. Hansen, James E. TI Prevented Mortality and Greenhouse Gas Emissions from Historical and Projected Nuclear Power SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID ELECTRICITY-GENERATION; CLIMATE-CHANGE; ENERGY; HEALTH; COAL AB In the aftermath of the March 2011 accident at Japan's Fukushima Daiichi nuclear power plant, the future contribution of nuclear power to the global energy supply has become somewhat uncertain. Because nuclear power is an abundant, low-carbon source of base-load power, it could make a large contribution to mitigation of global climate change and air pollution. Using historical production data, we calculate that global nuclear power has prevented an average of 1.84 million air pollution-related deaths and 64 gigatonnes of CO2-equivalent (GtCO(2)-eq) greenhouse gas (GHG) emissions that would have resulted from fossil fuel burning. On the basis of global projection data that take into account the effects of the Fukushima accident, we find that nuclear power could additionally prevent an average of 420 000-7.04 million deaths and 80-240 GtCO(2)-eq emissions due to fossil fuels by midcentury, depending on which fuel it replaces. By contrast, we assess that large-scale expansion of unconstrained natural gas use would not mitigate the climate problem and would cause far more deaths than expansion of nuclear power. C1 [Kharecha, Pushker A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Earth Inst, New York, NY 10025 USA. RP Kharecha, PA (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM pushker@giss.nasa.gov FU Lenfest Foundation; Columbia University-NASA Cooperative Agreement [NNX11AR63A] FX We thank Chuck Kutscher of the U.S. DOE National Renewable Energy Laboratory for helpful comments on our methodology and three anonymous reviewers for helpful feedback on our manuscript. Funding for this work was provided by the Lenfest Foundation and the Columbia University-NASA Cooperative Agreement (award NNX11AR63A). NR 35 TC 49 Z9 49 U1 8 U2 75 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD MAY 7 PY 2013 VL 47 IS 9 BP 4889 EP 4895 DI 10.1021/es3051197 PG 7 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 141WA UT WOS:000318756000116 PM 23495839 ER PT J AU Gangupomu, VK Wagner, JR Park, IH Jain, A Vaidehi, N AF Gangupomu, Vamshi K. Wagner, Jeffrey R. Park, In-Hee Jain, Abhinandan Vaidehi, Nagarajan TI Mapping Conformational Dynamics of Proteins Using Torsional Dynamics Simulations SO BIOPHYSICAL JOURNAL LA English DT Article ID CONSTRAINED MOLECULAR-DYNAMICS; GENERALIZED BORN MODEL; MAMBA SNAKE-VENOM; BIOMOLECULAR SIMULATIONS; CALMODULIN STRUCTURE; FORCE-FIELD; INDUCED-FIT; TRANSITIONS; ASSOCIATION; RESOLUTION AB All-atom molecular dynamics simulations are widely used to study the flexibility of protein conformations. However, enhanced sampling techniques are required for simulating protein dynamics that occur on the millisecond timescale. In this work, we show that torsional molecular dynamics simulations enhance protein conformational sampling by performing conformational search in the low-frequency torsional degrees of freedom. In this article, we use our recently developed torsional-dynamics method called Generalized Newton-Euler Inverse Mass Operator (GNEIMO) to study the conformational dynamics of four proteins. We investigate the use of the GNEIMO method in simulations of the conformationally flexible proteins fasciculin and calmodulin, as well as the less flexible crambin and bovine pancreatic trypsin inhibitor. For the latter two proteins, the GNEIMO simulations with an implicit-solvent model reproduced the average protein structural fluctuations and sample conformations similar to those from Cartesian simulations with explicit solvent. The application of GNEIMO with replica exchange to the study of fasciculin conformational dynamics produced sampling of two of this protein's experimentally established conformational substates. Conformational transition of calmodulin from the Ca2+-bound to the Ca2+-free conformation occurred readily with GNEIMO simulations. Moreover, the GNEIMO method generated an ensemble of conformations that satisfy about half of both short- and long-range interresidue distances obtained from NMR structures of holo to apo transitions in calmodulin. Although unconstrained all-atom Cartesian simulations have failed to sample transitions between the substates of fasciculin and calmodulin, GNEIMO simulations show the transitions in both systems. The relatively short simulation times required to capture these long-timescale conformational dynamics indicate that GNEIMO is a promising molecular-dynamics technique for studying domain motion in proteins. C1 [Gangupomu, Vamshi K.; Wagner, Jeffrey R.; Park, In-Hee; Vaidehi, Nagarajan] City Hope Natl Med Ctr, Beckman Res Inst, Div Immunol, Duarte, CA USA. [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Vaidehi, N (reprint author), City Hope Natl Med Ctr, Beckman Res Inst, Div Immunol, Duarte, CA USA. EM nvaidehi@coh.org FU NIGMS grant [R01-GM082896]; National Aeronautics and Space Administration FX We thank Dr. Paul Brazhnik of the National Institute of General Medical Sciences (NIGMS) for his support and encouragement. We thank Simbios, the National Institutes of Health Center for Biomedical Computation at Stanford University, for providing us with the GBSA solvation module. Part of the research described in this article was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; Funding for this work was provided by NIGMS grant R01-GM082896. NR 52 TC 7 Z9 7 U1 2 U2 22 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0006-3495 J9 BIOPHYS J JI Biophys. J. PD MAY 7 PY 2013 VL 104 IS 9 BP 1999 EP 2008 DI 10.1016/j.bpj.2013.01.050 PG 10 WC Biophysics SC Biophysics GA 141VJ UT WOS:000318754300021 PM 23663843 ER PT J AU Liu, D Hussey, D Gubarev, MV Ramsey, BD Jacobson, D Arif, M Moncton, DE Khaykovich, B AF Liu, D. Hussey, D. Gubarev, M. V. Ramsey, B. D. Jacobson, D. Arif, M. Moncton, D. E. Khaykovich, B. TI Demonstration of achromatic cold-neutron microscope utilizing axisymmetric focusing mirrors SO APPLIED PHYSICS LETTERS LA English DT Article ID GRAZING-INCIDENCE OPTICS; SCATTERING; LENS; INSTRUMENTATION; GUIDES AB An achromatic cold-neutron microscope with magnification 4 is demonstrated. The image-forming optics is composed of nested coaxial mirrors of full figures of revolution, so-called Wolter optics. The spatial resolution, field of view, and depth of focus are measured and found consistent with ray-tracing simulations. Methods of increasing the resolution and magnification are discussed, as well as the scientific case for the neutron microscope. In contrast to traditional pinhole-camera neutron imaging, the resolution of the microscope is determined by the mirrors rather than by the collimation of the beam, leading to possible dramatic improvements in the signal rate and resolution. (C) 2013 AIP Publishing LLC. C1 [Liu, D.; Moncton, D. E.; Khaykovich, B.] MIT, Nucl Reactor Lab, Cambridge, MA 02139 USA. [Hussey, D.; Jacobson, D.; Arif, M.] NIST, Phys Measurement Lab, Gaithersburg, MD 20899 USA. [Gubarev, M. V.; Ramsey, B. D.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Moncton, D. E.] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Liu, D (reprint author), MIT, Nucl Reactor Lab, 138 Albany St, Cambridge, MA 02139 USA. EM bkh@mit.edu RI Liu, Dazhi/G-2675-2013; Khaykovich, Boris/A-7376-2012 OI Liu, Dazhi/0000-0002-7604-6940; Khaykovich, Boris/0000-0002-9490-2771 FU U.S. Department of Energy, Office of Basic Energy Sciences, Division of Materials Sciences and Engineering [DE-FG02-09ER46556, DE-FG02-09ER46557]; U.S. Department of Commerce; NIST Radiation and Biomolecular Physics Division; Director's office of NIST; NIST Center for Neutron Research; Department of Energy [DE_AI01-01EE50660] FX The authors are grateful to the NCNR technical support staff, especially Eli Baltic and Danny Ogg and to R. G. Downing for the temporary use of NG-1 for these experiments. Research supported by the U.S. Department of Energy, Office of Basic Energy Sciences, Division of Materials Sciences and Engineering under Award Nos. DE-FG02-09ER46556 and DE-FG02-09ER46557. NIST authors acknowledge support from the U.S. Department of Commerce, the NIST Radiation and Biomolecular Physics Division, the Director's office of NIST, the NIST Center for Neutron Research, and the Department of Energy inter-agency Agreement No. DE_AI01-01EE50660. NR 39 TC 15 Z9 15 U1 3 U2 22 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 MAY 6 PY 2013 VL 102 IS 18 AR 183508 DI 10.1063/1.4804178 PG 5 WC Physics, Applied SC Physics GA 164VV UT WOS:000320439900086 ER PT J AU Borucki, WJ Agol, E Fressin, F Kaltenegger, L Rowe, J Isaacson, H Fischer, D Batalha, N Lissauer, JJ Marcy, GW Fabrycky, D Desert, JM Bryson, ST Barclay, T Bastien, F Boss, A Brugamyer, E Buchhave, LA Burke, C Caldwell, DA Carter, J Charbonneau, D Crepp, JR Christensen-Dalsgaard, J Christiansen, JL Ciardi, D Cochran, WD DeVore, E Doyle, L Dupree, AK Endl, M Everett, ME Ford, EB Fortney, J Gautier, TN Geary, JC Gould, A Haas, M Henze, C Howard, AW Howell, SB Huber, D Jenkins, JM Kjeldsen, H Kolbl, R Kolodziejczak, J Latham, DW Lee, BL Lopez, E Mullally, F Orosz, JA Prsa, A Quintana, EV Sanchis-Ojeda, R Sasselov, D Seader, S Shporer, A Steffen, JH Still, M Tenenbaum, P Thompson, SE Torres, G Twicken, JD Welsh, WF Winn, JN AF Borucki, William J. Agol, Eric Fressin, Francois Kaltenegger, Lisa Rowe, Jason Isaacson, Howard Fischer, Debra Batalha, Natalie Lissauer, Jack J. Marcy, Geoffrey W. Fabrycky, Daniel Desert, Jean-Michel Bryson, Stephen T. Barclay, Thomas Bastien, Fabienne Boss, Alan Brugamyer, Erik Buchhave, Lars A. Burke, Chris Caldwell, Douglas A. Carter, Josh Charbonneau, David Crepp, Justin R. Christensen-Dalsgaard, Jorgen Christiansen, Jessie L. Ciardi, David Cochran, William D. DeVore, Edna Doyle, Laurance Dupree, Andrea K. Endl, Michael Everett, Mark E. Ford, Eric B. Fortney, Jonathan Gautier, Thomas N., III Geary, John C. Gould, Alan Haas, Michael Henze, Christopher Howard, Andrew W. Howell, Steve B. Huber, Daniel Jenkins, Jon M. Kjeldsen, Hans Kolbl, Rea Kolodziejczak, Jeffery Latham, David W. Lee, Brian L. Lopez, Eric Mullally, Fergal Orosz, Jerome A. Prsa, Andrej Quintana, Elisa V. Sanchis-Ojeda, Roberto Sasselov, Dimitar Seader, Shawn Shporer, Avi Steffen, Jason H. Still, Martin Tenenbaum, Peter Thompson, Susan E. Torres, Guillermo Twicken, Joseph D. Welsh, William F. Winn, Joshua N. TI Kepler-62: A Five-Planet System with Planets of 1.4 and 1.6 Earth Radii in the Habitable Zone SO SCIENCE LA English DT Article ID SUN-LIKE STAR; TRANSITING PLANET; CANDIDATES; SCIENCE; MASS; II. AB We present the detection of five planets-Kepler-62b, c, d, e, and f-of size 1.31, 0.54, 1.95, 1.61 and 1.41 Earth radii (R-circle plus), orbiting a K2V star at periods of 5.7, 12.4, 18.2, 122.4, and 267.3 days, respectively. The outermost planets, Kepler-62e and -62f, are super-Earth-size (1.25 R-circle plus < planet radius <= 2.0 R-circle plus) planets in the habitable zone of their host star, respectively receiving 1.2 +/- 0.2 times and 0.41 +/- 0.05 times the solar flux at Earth's orbit. Theoretical models of Kepler-62e and -62f for a stellar age of similar to 7 billion years suggest that both planets could be solid, either with a rocky composition or composed of mostly solid water in their bulk. C1 [Borucki, William J.; Batalha, Natalie; Lissauer, Jack J.; Bryson, Stephen T.; Haas, Michael; Henze, Christopher; Howell, Steve B.; Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Agol, Eric; Lee, Brian L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Fressin, Francois; Kaltenegger, Lisa; Desert, Jean-Michel; Carter, Josh; Charbonneau, David; Dupree, Andrea K.; Geary, John C.; Latham, David W.; Sasselov, Dimitar; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaltenegger, Lisa] Max Planck Inst Astron, D-69115 Heidelberg, Germany. [Rowe, Jason; Burke, Chris; Caldwell, Douglas A.; Christiansen, Jessie L.; DeVore, Edna; Doyle, Laurance; Jenkins, Jon M.; Mullally, Fergal; Quintana, Elisa V.; Seader, Shawn; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA. [Isaacson, Howard; Marcy, Geoffrey W.; Kolbl, Rea] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Fischer, Debra] Yale Univ, New Haven, CT 06520 USA. [Fabrycky, Daniel; Fortney, Jonathan; Lopez, Eric; Shporer, Avi] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Fabrycky, Daniel] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Bastien, Fabienne] Vanderbilt Univ, Nashville, TN 37235 USA. [Boss, Alan] Carnegie Inst Sci, Washington, DC 20015 USA. [Brugamyer, Erik; Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Crepp, Justin R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, Aarhus, Denmark. [Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kolodziejczak, Jeffery] George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Orosz, Jerome A.; Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA. [Prsa, Andrej] Villanova Univ, Villanova, PA 19085 USA. [Shporer, Avi] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Steffen, Jason H.] Northwestern Univ, Evanston, IL 60208 USA. [Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Cambridge, MA 02139 USA. RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM william.j.borucki@nasa.gov RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; /0000-0002-0802-9145; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Fischer, Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; W. M. Keck Foundation; Deutsche Forschungsgemeinschaft [ENP Ka 3142/1-1]; NASA Astrobiology Institute; Danish National Research Foundation; ASTERISK project; European Research Council [267864]; NASA through the Kepler Participating Scientist Program (PSP); NSF [AST-1109928, AST-0645416]; NASA [ADAP12-0172]; NASA PSP [NNX08AR04G, NNX12AF73G]; NASA FX Kepler was competitively selected as the 10th Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership of the California Institute of Technology, the University of California, and NASA. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. L.K. acknowledges support from Deutsche Forschungsgemeinschaft grants ENP Ka 3142/1-1 and NASA Astrobiology Institute. Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation. The research is supported by the ASTERISK project (Asteroseismic Investigations with SONG and Kepler) funded by European Research Council grant 267864. W. F. W. and J.A.O. acknowledge support from NASA through the Kepler Participating Scientist Program (PSP) and from NSF grant AST-1109928. D.F. acknowledges support from NASA ADAP12-0172. O.R.S.-O. and J.N.W. are supported by the Kepler PSP through grant NNX12AC76G. E.F. is partially supported by NASA PSP grants NNX08AR04G and NNX12AF73G. E.A. acknowledges NSF career grant AST-0645416. We also thank the Spitzer staff at IPAC and in particular N. Silbermann for checking and scheduling the Spitzer observations. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We thank the many people who gave so generously of their time to make this mission a success. All data products are available to the public at the Mikulski Archive for Space Telescopes, http://stdatu.stsci.edu/kepler. NR 26 TC 98 Z9 99 U1 90 U2 290 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 MAY 3 PY 2013 VL 340 IS 6132 BP 587 EP 590 DI 10.1126/science.1234702 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 135EA UT WOS:000318268900042 PM 23599262 ER PT J AU Morgan, GA Campbell, BA Carter, LM Plaut, JJ Phillips, RJ AF Morgan, Gareth A. Campbell, Bruce A. Carter, Lynn M. Plaut, Jeffrey J. Phillips, Roger J. TI 3D Reconstruction of the Source and Scale of Buried Young Flood Channels on Mars SO SCIENCE LA English DT Article ID CERBERUS FOSSAE; STRATIGRAPHY; PLAINS; WATER; LAVA AB Outflow channels on Mars are interpreted as the product of gigantic floods due to the catastrophic eruption of groundwater that may also have initiated episodes of climate change. Marte Vallis, the largest of the young martian outflow channels (<500 million years old), is embayed by lava flows that hinder detailed studies and comparisons with older channel systems. Understanding Marte Vallis is essential to our assessment of recent Mars hydrologic activity during a period otherwise considered to be cold and dry. Using data from the Shallow Radar sounder on the Mars Reconnaissance Orbiter, we present a three-dimensional (3D) reconstruction of buried channels on Mars and provide estimates of paleohydrologic parameters. Our work shows that Cerberus Fossae provided the waters that carved Marte Vallis, and it extended an additional 180 kilometers to the east before the emplacement of the younger lava flows. We identified two stages of channel incision and determined that channel depths were more than twice those of previous estimates. C1 [Morgan, Gareth A.; Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO USA. RP Morgan, GA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM morganga@si.edu RI Carter, Lynn/D-2937-2012 FU NASA Mars Reconnaissance Orbiter Project FX C. Chazen and T. Watters provided very helpful reviews of earlier versions of the paper. Comments and suggestions by four anonymous referees were extremely beneficial. Thanks are also extended to P. Russell for his technical assistance. Funding for this work was provided by the NASA Mars Reconnaissance Orbiter Project. The SHARAD data and MOLA altimetry are available through NASA's Planetary Data system. NR 22 TC 5 Z9 5 U1 0 U2 24 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 3 PY 2013 VL 340 IS 6132 BP 607 EP 610 DI 10.1126/science.1234787 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 135EA UT WOS:000318268900047 PM 23470730 ER PT J AU Littenberg, TB Baker, JG Buonanno, A Kelly, BJ AF Littenberg, Tyson B. Baker, John G. Buonanno, Alessandra Kelly, Bernard J. TI Systematic biases in parameter estimation of binary black-hole mergers SO PHYSICAL REVIEW D LA English DT Article ID COMPACT BINARIES; GRAVITATIONAL-RADIATION; MASS; OBJECT; X-1 AB Parameter estimation of binary black-hole merger events in gravitational-wave data relies on matched-filtering techniques which, in turn, depend on accurate model waveforms. Here we characterize the systematic biases introduced in measuring astrophysical parameters of binary black holes by applying the currently most accurate effective-one-body templates to simulated data containing nonspinning numerical-relativity waveforms. We quantify the systematic bias by using a Markov chain Monte Carlo algorithm to sample the posterior distribution function of noise-free data, and compare the offset of the maximum a priori waveform parameters (the bias) to the width of the distribution, which we refer to as the statistical error. For advanced ground-based detectors, we find that the systematic biases are well within the statistical error for realistic signal-to-noise ratios. These biases grow to be comparable to the statistical errors at high ground-based-instrument signal-to-noise ratios (SNR similar to 50), but never dominate the error budget. At the much larger signal-to-noise ratios expected for space-based detectors, these biases will become large compared to the statistical errors, but for astrophysical black hole mass estimates the absolute biases (of at most a few percent) are still fairly small. C1 [Littenberg, Tyson B.; Buonanno, Alessandra] Univ Maryland, Maryland Ctr Fundamental Phys, Dept Phys, College Pk, MD 20742 USA. [Littenberg, Tyson B.; Buonanno, Alessandra] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Littenberg, Tyson B.; Baker, John G.; Kelly, Bernard J.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Kelly, Bernard J.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Kelly, Bernard J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. RP Littenberg, TB (reprint author), Univ Maryland, Maryland Ctr Fundamental Phys, Dept Phys, College Pk, MD 20742 USA. OI Kelly, Bernard/0000-0002-3326-4454 FU NASA [08-ATFP08-0126, 11-ATP11-0046, 09-ATP09-0136]; NSF [PHY-0903631, PHY-1208881]; National Science Foundation [PHY-0923409, PHY-0600953] FX We would like to thank Ryan Lang, Sean McWilliams, Yi Pan, and Ira Thorpe for very useful discussions. We also thank the Caltech-Cornell-CITA Collaboration for providing us with the NR waveforms used in this work. The authors acknowledge support from the NASA Grants No. 08-ATFP08-0126 and No. 11-ATP11-0046, and J. G. B. and B. J. K. also acknowledge support from Grant No. 09-ATP09-0136. A. B. also acknowledges support from the NSF Grants No. PHY-0903631 and No. PHY-1208881. The MCMC runs were carried out using resources from the NASA Center for Climate Simulation at Goddard Space Flight Center, and the Nemo cluster supported by National Science Foundation Grants No. PHY-0923409 and No. PHY-0600953 to UW-Milwaukee. NR 83 TC 22 Z9 22 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAY 2 PY 2013 VL 87 IS 10 AR 104003 DI 10.1103/PhysRevD.87.104003 PG 16 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 145GD UT WOS:000319002300001 ER PT J AU Paielli, RA AF Paielli, Russell A. TI Automated Generation of Air Traffic Encounters for Testing Conflict-Resolution Software SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article ID AIRSPACE AB A method was developed to automatically generate simulated air traffic encounters for testing conflict-resolution software. A trajectory scripting language was developed to generate simulated trajectories that result in conflicts with a specified geometry. A script was then written to automatically generate a set of scripts written in the trajectory language, each of which generates a conflict with a specified geometry involving two flights. A set of level-flight conflicts was generated by taking permutations of three basic encounter parameters: the path crossing angle, the minimum separation, and the aircraft speeds. A set of nonlevel-flight conflicts was also generated by varying the altitude difference and the vertical velocity difference at minimum separation. The resulting conflicts were then run with conflict resolution in a fast-time, batch-mode simulation of the resulting maneuvers. Plots of the resulting resolution maneuvers allow the algorithm developer to quickly visualize and verify the reasonableness of the maneuvers for a wide range of encounter geometries. The results can also help find errors in the conflict-resolution algorithm and software. C1 NASA, Ames Res Ctr, Aviat Syst Div, Moffett Field, CA 94035 USA. RP Paielli, RA (reprint author), NASA, Ames Res Ctr, Aviat Syst Div, Mailstop 210-10, Moffett Field, CA 94035 USA. EM Russ.Paielli@nasa.gov NR 16 TC 1 Z9 1 U1 1 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD MAY PY 2013 VL 10 IS 5 BP 209 EP 217 DI 10.2514/1.54104 PG 9 WC Engineering, Aerospace SC Engineering GA AB2FQ UT WOS:000331609000001 ER PT J AU Pattarini, JM Blue, RS Blair, SN Lee, DC Russell, S Sui, XM Johnston, SL AF Pattarini, James M. Blue, Rebecca S. Blair, Steven N. Lee, Duck-Chul Russell, Steven Sui, Xuemei Johnston, Smith L. TI Association between Isokinetic Muscular Strength and All-Cause Mortality in Males SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Meeting Abstract CT 60th Annual Meeting of the American-College-of-Sports-Medicine CY MAY 28-JUN 01, 2013 CL Indianapolis, IN SP Amer Coll Sports Med C1 [Pattarini, James M.; Blue, Rebecca S.] Univ Texas Med Branch, Galveston, TX 77555 USA. [Blair, Steven N.; Sui, Xuemei] Univ S Carolina, Columbia, SC 29208 USA. [Lee, Duck-Chul] Iowa State Univ, Ames, IA USA. [Russell, Steven] Injury Reduct Technol Inc, Pawleys Island, SC USA. [Johnston, Smith L.] NASA, Houston, TX USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0195-9131 EI 1530-0315 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD MAY PY 2013 VL 45 IS 5 SU 1 MA 1153 BP 259 EP 259 PG 1 WC Sport Sciences SC Sport Sciences GA 300ND UT WOS:000330469702103 ER PT J AU Irons, JR Leveland, TR AF Irons, James R. Leveland, Thomas R. TI Eighth Landsat Satellite Becomes Operational SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article C1 [Irons, James R.] LDCM, Greenbelt, MD 20771 USA. [Irons, James R.] NASA, Washington, DC USA. [Leveland, Thomas R.] USGS, USGS EROS Ctr, Garretson, SD USA. RP Irons, JR (reprint author), LDCM, Greenbelt, MD 20771 USA. EM james.r.irons@nasa.gov; loveland@usgs.gov NR 3 TC 6 Z9 6 U1 0 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 MAY PY 2013 VL 79 IS 5 BP 398 EP 401 PG 4 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 295BY UT WOS:000330092800001 ER PT J AU Naghipour, P Pineda, EJ Arnold, SM AF Naghipour, Paria Pineda, Evan J. Arnold, Steven M. TI A Novel Approach to Modeling of Interfacial Fiber/Matrix Cyclic Debonding SO CMC-COMPUTERS MATERIALS & CONTINUA LA English DT Article ID FIBER-REINFORCED COMPOSITES; TRANSFORMATION FIELD ANALYSIS; TRANSVERSE COMPRESSION; COHESIVE ZONE; DAMAGE; DELAMINATION; FAILURE; ELEMENT; SHEAR; FORMULATION AB The micromechanics theory, generalized method of cells (GMC), was employed to simulate the debonding of fiber/matrix interfaces, within a repeating unit cell subjected to global, cyclic loading, utilizing a cyclic crack growth law. Cycle dependent, interfacial debonding was implemented as a new module to the available GMC formulation. The degradation of interfacial stresses with applied load cycles was achieved via progressive evolution of the interfacial compliance A periodic repeating unit cell, representing the fiber/matrix architecture of a composite, was subjected to combined normal and shear loadings, and degradation of the global transverse stress in successive cycles was monitored. The obtained results were compared to values from a corresponding finite element model. Reasonable agreement was achieved for combined normal and shear loading conditions, with minimal variation for pure loading cases. The higher variation in mixed loading cases was attributed to the uncoupled normal/shear formulation of GMC, and can be further improved by using available high fidelity options. C1 [Naghipour, Paria] Ohio Aerosp Inst, Brookpark, OH USA. [Pineda, Evan J.; Arnold, Steven M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Naghipour, P (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Brookpark, OH USA. NR 41 TC 0 Z9 0 U1 0 U2 3 PU TECH SCIENCE PRESS PI NORCROSS PA 6825 JIMMY CARTER BLVD, STE 1850, NORCROSS, GA 30071 USA SN 1546-2218 EI 1546-2226 J9 CMC-COMPUT MATER CON JI CMC-Comput. Mat. Contin. PD MAY PY 2013 VL 35 IS 1 BP 17 EP 33 PG 17 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary; Mathematics, Interdisciplinary Applications SC Engineering; Materials Science; Mathematics GA 255GG UT WOS:000327226800003 ER PT J AU Liu, KC Arnold, SM AF Liu, K. C. Arnold, S. M. TI Influence of Scale Specific Features on the Progressive Damage of Woven Ceramic Matrix Composites (CMCs) SO CMC-COMPUTERS MATERIALS & CONTINUA LA English DT Article DE Micromechanics; Multiscale Modeling; Textile Composites; Woven Composites; Progressive Damage; Monte Carlo; Probabilistic Modeling ID MICROMECHANICAL ANALYSIS; CVISIC COMPOSITES; FIBER COMPOSITES; CELLS AB It is well known that failure of a material is a locally driven event. In the case of ceramic matrix composites (CMCs), significant variations in the microstructure of the composite exist and their significance on both deformation and life response need to be assessed. Examples of these variations include changes in the fiber tow shape, tow shifting/nesting and voids within and between tows. In the present work, the influence of many of these scale specific architectural features of woven ceramic composite are examined stochastically at both the macroscale (woven repeating unit cell (RUC)) and structural scale (idealized using multiple RUCs). The recently developed Multi Scale Generalized Method of Cells (MSGMC) methodology is used to determine the overall deformation response, proportional elastic limit (first matrix cracking), and failure under tensile loading conditions and associated probability distribution functions. Prior results showed that the most critical architectural parameter to account for is weave void shape and content with other parameters being less in severity. Current results show that statistically only the post-elastic limit region (secondary hardening modulus and ultimate tensile strength) is impacted by local uncertainties both at the macro and structural level. C1 [Liu, K. C.] Arizona State Univ, Tempe, AZ 85287 USA. [Arnold, S. M.] NASA, GRC, Cleveland, OH 44135 USA. RP Liu, KC (reprint author), Arizona State Univ, Tempe, AZ 85287 USA. NR 20 TC 4 Z9 4 U1 2 U2 6 PU TECH SCIENCE PRESS PI NORCROSS PA 6825 JIMMY CARTER BLVD, STE 1850, NORCROSS, GA 30071 USA SN 1546-2218 EI 1546-2226 J9 CMC-COMPUT MATER CON JI CMC-Comput. Mat. Contin. PD MAY PY 2013 VL 35 IS 1 BP 35 EP 65 PG 31 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary; Mathematics, Interdisciplinary Applications SC Engineering; Materials Science; Mathematics GA 255GG UT WOS:000327226800004 ER PT J AU Pineda, EJ Bednarcyk, BA Waas, AM Arnold, SM AF Pineda, Evan J. Bednarcyk, Brett A. Waas, Anthony M. Arnold, Steven M. TI Progressive failure of a unidirectional fiber-reinforced composite using the method of cells: Discretization objective computational results SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES LA English DT Article DE Polymer-matrix composites; Multiscale modeling; Fracture; Computational mechanics; Cohesive Failure ID PERIODIC MULTIPHASE MATERIALS; FINITE-ELEMENT ANALYSIS; CRACK BAND PROPAGATION; HIGHER-ORDER THEORY; TRANSVERSE COMPRESSION; PHENOMENOLOGICAL MODELS; DAMAGE MECHANICS; MICROMECHANICS; DEFORMATION; MATRIX AB The smeared crack band theory is implemented within the high-fidelity generalized method of cells micromechanics model to capture progressive failure within the constituents of a composite material while retaining objectivity with respect to the size of the discretization elements used in the model. Orientation of the crack band is determined using the maximum principal stress. When oriented perpendicular to the maximum principle stress the faces of the cracks in the crack band are subjected to only normal tractions and grow under pure mode I conditions. The traction-separation law governing the behavior of the crack band is related to the mode I fracture toughness, and formation of the crack band is initiated with a maximum stress criterion. Conversely, if the direction of the principal stress with the largest magnitude is compressive, it is assumed that the cracks within the crack band are constrained from growing in mode I. Instead, it is assumed that mode II cracks form within the crack band oriented along the plane of maximum shear stress. A Mohr-Coulomb initiation criterion is utilized to incorporate the effects of the normal tractions acting on the crack faces, and an effective shear traction is defined accordingly. The effective shear traction versus mode II separation law is a function of the mode II fracture toughness. A repeating unit cell containing 13 randomly arranged fibers is modeled and subjected to a combination of transverse tension/compression and transverse shear loading. The implementation is verified against experimental data and an equivalent finite element model that utilizes the same implementation of the crack band theory. Additionally, a sensitivity study is also performed on the effect of the size of the RUC on the stiffness and strength of the RUC. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Pineda, Evan J.; Bednarcyk, Brett A.; Arnold, Steven M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Waas, Anthony M.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Waas, AM (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA. EM dcw@umich.edu NR 54 TC 16 Z9 16 U1 0 U2 15 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7683 EI 1879-2146 J9 INT J SOLIDS STRUCT JI Int. J. Solids Struct. PD MAY 1 PY 2013 VL 50 IS 9 BP 1203 EP 1216 DI 10.1016/j.ijsolstr.2012.12.003 PG 14 WC Mechanics SC Mechanics GA 250MZ UT WOS:000326858200002 ER PT J AU Davies, AG Chien, S Doubleday, J Tran, D Thordarson, T Gudmundsson, MT Hoskuldsson, A Jakobsdottir, SS Wright, R Mandl, D AF Davies, Ashley Gerard Chien, Steve Doubleday, Joshua Tran, Daniel Thordarson, Thorvaldur Gudmundsson, Magnus T. Hoskuldsson, Armann Jakobsdottir, Steinunn S. Wright, Robert Mandl, Daniel TI Observing Iceland's Eyjafjallajokull 2010 eruptions with the autonomous NASA Volcano Sensor Web SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE volcanoes; autonomy; remote sensing; sensor web ID SCIENCECRAFT EXPERIMENT; SATELLITE DATA; HYPERION; SPACE; TIME; EO-1 AB Between 24 March and 5 June 2010, the Hyperion hyperspectral imager and Advanced Land Imager (ALI) on NASA's Earth Observing 1 (EO-1) spacecraft obtained an unprecedented sequence of 50 observation pairs of the eruptions at Fimmvorouhals and Eyjafjallajokull, Iceland. This high acquisition rate was possible only through the use of data flow streamlined by using the autonomously operating NASA Volcano Sensor Web (VSW). The VSW incorporates notifications of volcanic activity from multiple sources to retask EO-1 and process Hyperion data to extract eruption parameters from high spatial and spectral resolution visible and short-wavelength infrared data. Physical changes in eruption style and magnitude were charted as the eruptions ran their course. Rapid data downlink and automatic data-processing algorithms generated a variety of products which are compared with estimates from ground-based observations and post-eruption in situ measurements. Estimates of effusion rate from heat loss measurements underestimate actual effusion rate (while still following broad eruption rate trends) but are closer to in situ estimates for effusive eruptions (Fimmvorouhals) than explosive, ash-rich eruptions (Eyjafjallajokull). During the later stages of the 2010 eruption, VSW-generated products were rapidly delivered to end-users in Iceland to aid in the assessment of risk and hazard. The success of the VSW led to Icelandic Meteorological Office (IMO) in situ sensors being incorporated into the VSW, and in May 2011 an IMO seismic alert autonomously triggered EO-1 observations of a new eruption at Grimsvotn volcano. Finally, the VSW demonstrates an autonomy-driven, multi-asset, spacecraft retasking and data processing system that maximizes science return, a desirable capability for future NASA missions. C1 [Davies, Ashley Gerard; Chien, Steve; Doubleday, Joshua; Tran, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Thordarson, Thorvaldur] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. [Thordarson, Thorvaldur; Gudmundsson, Magnus T.; Hoskuldsson, Armann] Univ Iceland, Inst Earth Sci, Reykjavik, Iceland. [Jakobsdottir, Steinunn S.] Iceland Meteorol Off, Reykjavik, Iceland. [Wright, Robert] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Mandl, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Davies, AG (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91040 USA. EM Ashley.Davies@jpl.nasa.gov RI Thordarson, Thorvaldur/M-2422-2015; Gudmundsson, Magnus/M-3735-2015 OI Thordarson, Thorvaldur/0000-0003-4011-7185; Gudmundsson, Magnus/0000-0001-5325-3368 FU NASA; NERC Emergency Grant [Ne/I00775x/1] FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. (c) 2013 Caltech. All rights reserved. Earth Observing 1 is managed by the NASA Goddard Space Flight Center, Greenbelt, Maryland, USA. T. Thordarson's contribution to this project was supported by NERC Emergency Grant (Ne/I00775x/1). The authors thank Michael Ramsey, Gaetana Ganci, and David Rothery for their detailed and extremely useful reviews of the manuscript, and Alison Canning Davies for her meticulous review of the proofs. NR 42 TC 3 Z9 3 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD MAY PY 2013 VL 118 IS 5 BP 1936 EP 1956 DI 10.1002/jgrb.50141 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 256HH UT WOS:000327299800041 ER PT J AU Gazeaux, J Williams, S King, M Bos, M Dach, R Deo, M Moore, AW Ostini, L Petrie, E Roggero, M Teferle, FN Olivares, G Webb, FH AF Gazeaux, Julien Williams, Simon King, Matt Bos, Machiel Dach, Rolf Deo, Manoj Moore, Angelyn W. Ostini, Luca Petrie, Elizabeth Roggero, Marco Teferle, Felix Norman Olivares, German Webb, Frank H. TI Detecting offsets in GPS time series: First results from the detection of offsets in GPS experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE GPS; offsets detection; homogenization; velocity ID CHANGE-POINTS; SEGMENTATION; SELECTION; MODELS AB The accuracy of Global Positioning System (GPS) time series is degraded by the presence of offsets. To assess the effectiveness of methods that detect and remove these offsets, we designed and managed the Detection of Offsets in GPS Experiment. We simulated time series that mimicked realistic GPS data consisting of a velocity component, offsets, white and flicker noises (1/f spectrum noises) composed in an additive model. The data set was made available to the GPS analysis community without revealing the offsets, and several groups conducted blind tests with a range of detection approaches. The results show that, at present, manual methods (where offsets are hand picked) almost always give better results than automated or semiautomated methods (two automated methods give quite similar velocity bias as the best manual solutions). For instance, the fifth percentile range (5% to 95%) in velocity bias for automated approaches is equal to 4.2mm/year (most commonly 0.4mm/yr from the truth), whereas it is equal to 1.8mm/yr for the manual solutions (most commonly 0.2mm/yr from the truth). The magnitude of offsets detectable by manual solutions is smaller than for automated solutions, with the smallest detectable offset for the best manual and automatic solutions equal to 5mm and 8mm, respectively. Assuming the simulated time series noise levels are representative of real GPS time series, robust geophysical interpretation of individual site velocities lower than 0.2-0.4mm/yr is therefore certainly not robust, although a limit of nearer 1mm/yr would be a more conservative choice. Further work to improve offset detection in GPS coordinates time series is required before we can routinely interpret submm/yr velocities for single GPS stations. Key Points Manual and automatic GPS offset detection methods are testedManual approaches yield smaller velocity biasesCare must be taken when interpreting single-site velocities <1mm/yr C1 [Gazeaux, Julien; King, Matt; Petrie, Elizabeth] Newcastle Univ, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Williams, Simon] Natl Oceanog Ctr, Liverpool, Merseyside, England. [King, Matt] Univ Tasmania, Sch Geog & Environm Studies, Hobart, Tas, Australia. [Bos, Machiel] Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, P-4100 Oporto, Portugal. [Dach, Rolf; Ostini, Luca] Univ Bern, Astron Inst, Bern, Switzerland. [Deo, Manoj] Natl Geospatial Reference Syst, Earth Monitoring Grp, Canberra, ACT, Australia. [Moore, Angelyn W.; Webb, Frank H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Roggero, Marco] Politecn Torino, Turin, Italy. [Teferle, Felix Norman; Olivares, German] Univ Luxembourg, Geophys Lab, Luxembourg, Luxembourg. RP Gazeaux, J (reprint author), Newcastle Univ, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. EM julien.gazeaux@ncl.ac.uk RI Petrie, Elizabeth (Liz)/B-8532-2008; Williams, Simon/C-7214-2011; Bos, Machiel/C-5486-2012; Scientific output, CIIMAR/E-5122-2012; King, Matt/B-4622-2008; Roggero, Marco/J-9071-2016 OI Petrie, Elizabeth (Liz)/0000-0002-7124-2600; Williams, Simon/0000-0003-4123-4973; Bos, Machiel/0000-0002-1946-8637; Scientific output, CIIMAR/0000-0001-6270-2153; King, Matt/0000-0001-5611-9498; Roggero, Marco/0000-0003-4950-6363 FU Leverhulme Trust; NERC; COST Action [ES0701]; National Aeronautics and Space Administration; Australian Research Council [FT110100207] FX This research was supported by the Leverhulme Trust, NERC, and COST Action ES0701. We thank Olivier Mestre and Mark Tamisiea for helpful discussions and the solution providers who elected not to be named as co-authors on this paper. We acknowledge SOPAC for making their offset information available. The research of the JPL authors was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Matt King is a recipient of an Australian Research Council Future Fellowship (project number FT110100207). NR 37 TC 27 Z9 28 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD MAY PY 2013 VL 118 IS 5 BP 2397 EP 2407 DI 10.1002/jgrb.50152 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 256HH UT WOS:000327299800010 ER PT J AU Getirana, ACV Paiva, RCD AF Getirana, Augusto C. V. Paiva, Rodrigo C. D. TI Mapping large- scale river flow hydraulics in the Amazon Basin SO WATER RESOURCES RESEARCH LA English DT Article DE flood wave; Saint-Venant equations; Amazon Basin; Froude number; time to peak ID LAG TIME; CLIMATE; MODEL; PARAMETERIZATIONS; WETLANDS; LAKES AB Key Points first attempt to map river flow dynamics in the Amazon basin new empirical equation for time of peak of flood waves designed for large rivers the map has a percentage of detection of 83.4% Research on actual requirements for a numerically consistent representation of flow dynamics in large-scale river-flood models are needed to improve both modeling performance and computational efficiency. Still, regional- and global-scale characterizations of river hydrodynamics are absent. A first attempt to map river hydrodynamics in the Amazon Basin is presented. Flood wave type maps at 0.25 degrees spatial resolution are derived from a classification method based on the analysis of Saint-Venant equation terms. Global river geometry data sets derived from both digital elevation models and empirical equations supported by stream gauge observations are used as input variables. Errors of input variables are estimated, and a sensitivity analysis is performed. Results show that 64.5% of rivers (headwaters and high-slope rivers) can be represented by the kinematic wave (KI), 34.5% (main Amazon tributaries, low slope, and wetland regions) by the diffusive wave (DF), and 1% (lower Amazon) by the full Saint-Venant equations (SV). In a rigorous scenario, i.e., a case where the most restricted classification of each grid cell is considered, approximate to 33% is classified as KI, approximate to 62% as DF, and approximate to 5% as SV. Most of the basin presents subcritical flow with very low Froude number (Fr), while the Andean region is dominated by larger Fr values and supercritical flow can be found. According to our evaluation mostly based on in situ data, the map has a percentage of detection of 83.4%. C1 [Getirana, Augusto C. V.] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Paiva, Rodrigo C. D.] Univ Fed Rio Grande do Sul, Inst Pesquisas Hidraul, Porto Alegre, RS, Brazil. [Paiva, Rodrigo C. D.] Univ Toulouse 3, Geosci Environm Toulouse, UMR 5563, F-31062 Toulouse, France. RP Getirana, ACV (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM augusto.getirana@nasa.gov RI Getirana, Augusto/A-6146-2010; Getirana, Augusto/G-4630-2011; OI Paiva, Rodrigo/0000-0003-2918-6681 FU CNPq (Conselho Nacional de Desenvolvimento Cientifico, Brazil) FX R.P. is funded by CNPq (Conselho Nacional de Desenvolvimento Cientifico, Brazil). Grateful acknowledgments are due to D. Yamazaki for providing FLOW algorithm outputs and to W. Collischonn (IPH/UFRGS), M. Trigg (U. Bristol), P. Bates (U. Bristol), and three anonymous reviewers for their valuable comments. This study benefited from data made available by ANA. NR 40 TC 1 Z9 1 U1 4 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD MAY PY 2013 VL 49 IS 5 BP 2437 EP 2445 DI 10.1002/wrcr.20212 PG 9 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 216OD UT WOS:000324292300009 ER PT J AU Yong, B Ren, LL Hong, Y Gourley, JJ Tian, YD Huffman, GJ Chen, X Wang, WG Wen, YX AF Yong, Bin Ren, Liliang Hong, Yang Gourley, Jonathan J. Tian, Yudong Huffman, George J. Chen, Xi Wang, Weiguang Wen, Yixin TI First evaluation of the climatological calibration algorithm in the real- time TMPA precipitation estimates over two basins at high and low latitudes SO WATER RESOURCES RESEARCH LA English DT Article DE satellite rainfall; validation; hydrology ID PRODUCTS; RAINFALL; DATASETS AB Key Points The crucial upgrade of TMPA-RT effectively reduces the systematic errors. This upgrade tends to perform worse at higher latitudes, especially in winter. Future efforts include improved error structure and extension to high latitudes. The TRMM Multi-satellite Precipitation Analysis (TMPA) system underwent a crucial upgrade in early 2009 to include a climatological calibration algorithm (CCA) to its real-time product 3B42RT, and this algorithm will continue to be applied in the future Global Precipitation Measurement era constellation precipitation products. In this study, efforts are focused on the comparison and validation of the Version 6 3B42RT estimates before and after the climatological calibration is applied. The evaluation is accomplished using independent rain gauge networks located within the high-latitude Laohahe basin and the low-latitude Mishui basin, both in China. The analyses indicate the CCA can effectively reduce the systematic errors over the low-latitude Mishui basin but misrepresent the intensity distribution pattern of medium-high rain rates. This behavior could adversely affect TMPA's hydrological applications, especially for extreme events (e.g., floods and landslides). Results also show that the CCA tends to perform slightly worse, in particular, during summer and winter, over the high-latitude Laohahe basin. This is possibly due to the simplified calibration-processing scheme in the CCA that directly applies the climatological calibrators developed within 40 degrees latitude to the latitude belts of 40 degrees N-50 degrees N. Caution should therefore be exercised when using the calibrated 3B42RT for heavy rainfall-related flood forecasting (or landslide warning) over high-latitude regions, as the employment of the smooth-fill scheme in the CCA bias correction could homogenize the varying rainstorm characteristics. Finally, this study highlights that accurate detection and estimation of snow at high latitudes is still a challenging task for the future development of satellite precipitation retrievals. C1 [Yong, Bin; Ren, Liliang; Chen, Xi; Wang, Weiguang] Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, Nanjing 210098, Jiangsu, Peoples R China. [Yong, Bin; Hong, Yang; Wen, Yixin] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Gourley, Jonathan J.] NOAA, Natl Severe Storms Lab, Off Ocean & Atmospher Res, Norman, OK 73069 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Tian, Yudong] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. [Huffman, George J.] Sci Syst & Applicat Inc, Greenbelt, MD USA. [Huffman, George J.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Yong, B (reprint author), Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, Nanjing 210098, Jiangsu, Peoples R China. EM yongbin_hhu@126.com RI Hong, Yang/D-5132-2009; Yong, Bin/C-2257-2014; Huffman, George/F-4494-2014; Gourley, Jonathan/C-7929-2016 OI Hong, Yang/0000-0001-8720-242X; Yong, Bin/0000-0003-1466-2091; Huffman, George/0000-0003-3858-8308; Gourley, Jonathan/0000-0001-7363-3755 FU National Natural Science Foundation of China [51190090]; 111 Project [B08048]; Natural Science Foundation of Jiangsu Province [BK2012813]; Open Research Fund of Key Laboratory of Digital Earth; Center for Earth Observation and Digital Earth; Chinese Academy of Sciences [2011LDE008]; Special Basic Research Fund for Methodology in Hydrology [2011IM011000]; Qinglan Project of Jiangsu Province; Open Fund of State Key Laboratory of Hydrology-Water Resources and Hydraulic Engineering [2012490111] FX The TMPA data used in this study were provided by the NASA/Goddard Space Flight Center's Laboratory for Atmospheres and PPS, which develop and compute the TMPA as a contribution to TRMM. The authors thank three anonymous reviewers who helped to improve the earlier version of this paper. This work was financially supported by the Major Program of National Natural Science Foundation of China (51190090) and the 111 Project (B08048). Also, this work is partially sponsored by Natural Science Foundation of Jiangsu Province (BK2012813), Open Research Fund of Key Laboratory of Digital Earth, Center for Earth Observation and Digital Earth, Chinese Academy of Sciences (2011LDE008), Special Basic Research Fund for Methodology in Hydrology (2011IM011000), Qinglan Project of Jiangsu Province, and Open Fund of State Key Laboratory of Hydrology-Water Resources and Hydraulic Engineering (2012490111). NR 26 TC 16 Z9 18 U1 2 U2 27 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD MAY PY 2013 VL 49 IS 5 BP 2461 EP 2472 DI 10.1002/wrcr.20246 PG 12 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 216OD UT WOS:000324292300011 ER PT J AU Sarazin, CL Finoguenov, A Wik, DR AF Sarazin, C. L. Finoguenov, A. Wik, D. R. TI Merger shocks in Abell 3667 and the Cygnus A cluster SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on Galaxy Clusters as Giant Cosmic Laboratories CY MAY 21-23, 2012 CL Madrid, SPAIN DE galaxies: clusters: general; galaxies: clusters: individual (Abell 3667, Cygnus A); intergalactic medium; shock waves; X-rays: galaxies: clusters ID X-RAY; A3667; GALAXIES AB We present new XMM-Newton observations of the northwest (NW) radio relic region in the cluster Abell 3667. We detect a jump in the X-ray surface brightness and X-ray temperature at the sharp outer edge of the radio relic which indicate that this is the location of a merger shock with a Mach number of about 2. Comparing the radio emission to the shock properties implies that approximately 0.2% of the dissipated shock kinetic energy goes into accelerating relativistic electrons. This is an order of magnitude smaller than the efficiency of shock acceleration in many Galactic supernova remnants, which may be due to the lower Mach numbers of cluster merger shocks. The X-ray and radio properties indicate that the magnetic field strength in the radio relic is greater than or similar to 3 mu G, which is a very large field at a projected distance of similar to 2.2 Mpc from the center of a cluster. The radio spectrum is relatively flat at the shock, and steepens dramatically with distance behind the shock. This is consistent with radiative losses by the electrons and the post-shock speed determined from the X-ray properties. The Cygnus Lambda radio source is located in a merging cluster of galaxies. This appears to be an early-stage merger. Our recent Suzaku observation confirm the presence of a hot region between the two subclusters which agrees with the predicted shocked region. The high spectral resolution of the CCDs on Suzaku allowed us to measure the radial component of the merger velocity, Delta nu(r) approximate to 2650 km s(-1). (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Finoguenov, A.] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland. [Finoguenov, A.] Univ Maryland Baltimore Cty, Ctr Space Sci Technol, Baltimore, MD 21250 USA. [Wik, D. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Sarazin, CL (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. EM sarazin@virginia.edu RI XRAY, SUZAKU/A-1808-2009 FU European Commission; NASA ADAP [NNX11AD15G]; NASA [NNX09AH25G, GO1-12169X] FX CLS thanks the Institute for Astro- and Particle Physics at the University of Innsbruck and the Eramus Mundus Program of the European Commission for their hospitality and support. This work was primarily funded by NASA ADAP Grant NNX11AD15G and NASA Suzaku Grant NNX09AH25G, but also by Chandra Grant GO1-12169X. NR 12 TC 8 Z9 8 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAY PY 2013 VL 334 IS 4-5 SI SI BP 346 EP 349 DI 10.1002/asna.201211854 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237IF UT WOS:000325862000009 ER PT J AU Zheng, W Bradley, L Zitrin, A Moustakas, J Postman, M Ford, H Shu, X Coe, D Moustakas, LA Koekemoer, A Milino, A Jouvel, S Host, O Broadhurst, T Kelson, DD AF Zheng, W. Bradley, L. Zitrin, A. Moustakas, J. Postman, M. Ford, H. Shu, X. Coe, D. Moustakas, L. A. Koekemoer, A. Milino, A. Jouvel, S. Host, O. Broadhurst, T. Kelson, D. D. TI Progress in search for high-redshift galaxies magnified by gravitational lensing SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on Galaxy Clusters as Giant Cosmic Laboratories CY MAY 21-23, 2012 CL Madrid, SPAIN DE early Universe; galaxies: high-redshift; galaxies: clusters: general; gravitational lensing; surveys ID EARLY RELEASE SCIENCE; LUMINOSITY FUNCTIONS; WFC3/IR OBSERVATIONS; MACS; CONSTRAINTS; DISCOVERY; CLUSTERS; UNIVERSE; HUDF09; END AB Our searches in the CLASH data have found many high-redshift galaxy candidates. One object at z = 6.2 in MACS J0329-02 is quadruply lensed. Another object in MACS J1149+ 22 is at redshift z = 9.6 and AB=25.7, the first candidate at z > 9 that is bright enough for spectroscopic observations. The discovery of more than 80 galaxy candidates at z > 7 demonstrates the unique potential of galaxy cluster fields for finding highly magnified, intrinsically faint galaxies at the highest redshifts. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Zheng, W.; Ford, H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bradley, L.; Postman, M.; Coe, D.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Zitrin, A.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Shu, X.] Univ Sci & Technol China, Dept Astron, Hefei 230026, Anhui, Peoples R China. [Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Milino, A.] Inst Astrofis Andalucia, E-18008 Granada, Spain. [Jouvel, S.; Host, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Broadhurst, T.] Univ Basque Country, Dept Theoret Phys, Bilbao 48080, Spain. [Kelson, D. D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Zheng, W (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM zheng@pha.jhu.edu RI Shu, Xinwen/D-7294-2017; OI Koekemoer, Anton/0000-0002-6610-2048; Shu, Xinwen/0000-0002-7020-4290; Moustakas, Leonidas/0000-0003-3030-2360 FU NASA [NAS 5-26555]; NASA through JPL/Caltech; Baden Wurttemberg Stiftung; NSF [AST-0908246] FX The CLASH Multi-Cycle Treasury Program (GO-12065) is based on observations made with the NASA/ESA Hubble Space Telescope. The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. A. J. is supported by contract research "Internationale Spitzenforschung II-1" of the Baden Wurttemberg Stiftung. J. M. acknowledges support from NSF grant AST-0908246. NR 21 TC 1 Z9 1 U1 2 U2 8 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAY PY 2013 VL 334 IS 4-5 SI SI BP 474 EP 477 DI 10.1002/asna.201211884 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237IF UT WOS:000325862000038 ER PT J AU Bruna, D Turner, MG AF Bruna, Dario Turner, Mark G. TI Isothermal Boundary Condition at Casing Applied to the Rotor 37 Transonic Axial Flow Compressor SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME LA English DT Article AB Computational fluid dynamics (CFD) simulations are presented with an isothermal boundary condition at the casing for running NASA Rotor 37. The casing temperature is set to the inlet total temperature. Relative to the adiabatic simulations, the comparison to experimental efficiency is much improved for the 100% speed line. The efficiency difference between the isothermal and adiabatic solutions is about 1%, and matches the low-flow test condition. The profiles of total temperature with the isothermal boundary condition match the data near the casing. The adiabatic simulation has a total temperature overshoot that has been consistently part of any data comparison of CFD with this data set, and is typical of most compressor calculations. The efficiency profile has a similar improvement in matching the data because of its relationship to temperature. The real rig is not isothermal at the casing and may require more complex simulations such as a conjugate heat transfer approach to truly match the physics. However, the isothermal boundary condition is more accurate and more realistic than the adiabatic boundary condition. C1 [Bruna, Dario] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Turner, Mark G.] Univ Cincinnati, Cincinnati, OH USA. RP Bruna, D (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM dariobruna@fastwebnet.it; mark.turner@uc.edu FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Glenn Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 9 TC 2 Z9 2 U1 1 U2 4 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0889-504X EI 1528-8900 J9 J TURBOMACH JI J. Turbomach.-Trans. ASME PD MAY PY 2013 VL 135 IS 3 AR 034501 DI 10.1115/1.4007569 PG 4 WC Engineering, Mechanical SC Engineering GA 239KD UT WOS:000326021300036 ER PT J AU Luchinsky, DG Hafiychuk, V Smelyanskiy, VN Kessler, S Walker, J Miller, J Watson, M AF Luchinsky, Dmitry G. Hafiychuk, Vasyl Smelyanskiy, Vadim N. Kessler, Seth Walker, James Miller, Jim Watson, Michael TI Modeling wave propagation and scattering from impact damage for structural health monitoring of composite sandwich plates SO STRUCTURAL HEALTH MONITORING-AN INTERNATIONAL JOURNAL LA English DT Article DE Honeycomb sandwich plates; waves scattering; impact behavior; delamination; nondestructive testing ID BEAMS AB Results of modeling of the wave propagation, impact, and damage detection in a sandwich honeycomb plate using piezoelectric actuator/sensor scheme are reported. A finite element model of honeycomb sandwich panel that reproduces accurately experimental setup and takes into account main characteristic features of the real composite panel, impactor, lead zirconate titanate actuator, and sensors is developed. The impact is simulated to obtain damage with parameters close to those observed in the experiment. Both in simulations and in experiment, the voltage signal of a given shape is applied to the lead zirconate titanate actuators to excite acoustic wave, and the electrical signals collected from the lead zirconate titanate sensors mounted to the panel are used to study wave propagation in the sandwich panel. The results of simulation are shown to be in good agreement with the experimental results both before and after the impact. Properties of acoustic wave propagating in composite sandwich honeycomb panels are discussed. C1 [Luchinsky, Dmitry G.] Mission Crit Technol Inc, El Segundo, CA USA. [Luchinsky, Dmitry G.; Hafiychuk, Vasyl; Smelyanskiy, Vadim N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hafiychuk, Vasyl] SGT Inc, Greenbelt, MD USA. [Kessler, Seth] Metis Design Corp, Cambridge, MA USA. [Walker, James; Miller, Jim; Watson, Michael] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Hafiychuk, V (reprint author), NASA, Ames Res Ctr, Mail Stop 269-2, Moffett Field, CA 94035 USA. EM vasyl.hafiychuk@nasa.gov NR 26 TC 3 Z9 3 U1 1 U2 14 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1475-9217 EI 1741-3168 J9 STRUCT HEALTH MONIT JI Struct. Health Monit. PD MAY PY 2013 VL 12 IS 3 BP 296 EP 308 DI 10.1177/1475921713483351 PG 13 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 236QC UT WOS:000325813100009 ER PT J AU Kwok, R Spreen, G Pang, S AF Kwok, R. Spreen, G. Pang, S. TI Arctic sea ice circulation and drift speed: Decadal trends and ocean currents SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE Arctic Ocean; sea ice; ice drift; circulation; trends; current ID NORTH-ATLANTIC OSCILLATION; MOTION AB We examine the basinwide trends in sea ice circulation and drift speed and highlight the changes between 1982 and 2009 in connection to regional winds, multiyear sea ice coverage, ice export, and the thinning of the ice cover. The polarity of the Arctic Oscillation (AO) is used as a backdrop for summarizing the variance and shifts in decadal drift patterns. The 28-year circulation fields show a net strengthening of the Beaufort Gyre and the Transpolar Drift, especially during the last decade. The imprint of the arctic dipole anomaly on the mean summer circulation is evident (2001-2009) and enhances summer ice area export at the Fram Strait. Between 2001 and 2009, the large spatially averaged trends in drift speeds (winter: +23.6%/decade, summer: +17.7%/decade) are not explained by the much smaller trends in wind speeds (winter: 1.46%/decade, summer: -3.42%/decade). Notably, positive trends in drift speed are found in regions with reduced multiyear sea ice coverage. Over 90% of the Arctic Ocean has positive trends in drift speed and negative trends in multiyear sea ice coverage. The increased responsiveness of ice drift to geostrophic wind is consistent with a thinner and weaker seasonal ice cover and suggests large-scale changes in the air-ice-ocean momentum balance. The retrieved mean ocean current field from decadal-scale average ice motion captures a steady drift from Siberia to the Fram Strait, an inflow north of the Bering Strait, and a westward drift along coastal Alaska. This mean current is comparable to geostrophic currents from satellite-derived dynamic topography. C1 [Kwok, R.; Spreen, G.; Pang, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ronald.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008; Spreen, Gunnar/A-4533-2010 OI Kwok, Ron/0000-0003-4051-5896; Spreen, Gunnar/0000-0003-0165-8448 FU National Aeronautics and Space Administration FX We thank M. Steele and J. Morison (University of Washington) for helpful discussions regarding the interpretation of the ocean currents. The SMMR and SSM/I data sets were provided by the National Snow and Ice Data Center, University of Colorado, Boulder, Colorado. The QuikSCAT data were provided by the Physical Oceanography DAAC at the Jet Propulsion Laboratory, Pasadena, California. R. K., G. S., and S. P. carried out this work at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 39 TC 63 Z9 64 U1 6 U2 44 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD MAY PY 2013 VL 118 IS 5 BP 2408 EP 2425 DI 10.1002/jgrc.20191 PG 18 WC Oceanography SC Oceanography GA 224TZ UT WOS:000324913700012 ER PT J AU Xie, HJ Tekeli, AE Ackley, SF Yi, DH Zwally, HJ AF Xie, Hongjie Tekeli, Ahmet Emre Ackley, Stephen F. Yi, Donghui Zwally, H. Jay TI Sea ice thickness estimations from ICESat Altimetry over the Bellingshausen and Amundsen Seas, 2003-2009 SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE sea ice freeboard; AMSR-E snow depth; empirical equation; buoyancy equation ID WEDDELL-SEA; SNOW-COVER; TEMPERATURE; ANTARCTICA; FREEBOARD; RADAR; DEPTH AB Sea ice thicknesses derived from NASA's Ice, Cloud, and Land Elevation Satellite (ICESat) altimetry data are examined using two different approaches, buoyancy and empirical equations, and at two spatial scalesICESat footprint size (70m diameter spot) and Advanced Microwave Scanning Radiometer (AMSR-E) pixel size (12.5km by 12.5km) for the Bellingshausen and Amundsen Seas of west Antarctica. Ice thickness from the empirical equation shows reasonable spatial and temporal distribution of ice thickness from 2003 to 2009. Ice thickness from the buoyancy equation, however, additionally needing snow depth information derived from the AMSR-E, shows an overestimation in terms of maximum, mean (+63% to 75%), and standard deviation while underestimation in modal thickness (-20%) as compared with those from the empirical equation approach. When ICESat snow freeboard is used as the snow depth in the buoyancy equation, i.e., the zero ice freeboard assumption, the derived ice thicknesses match well with those from the empirical equation approach, within 5% overall. The AMSR-E, therefore, may underestimate snow depth and accounts for similar to 95% of the ice thickness overestimation as compared with the buoyancy approach. The empirical equation derived ice thickness shows a consistent asymmetrical distribution with a long tail to high values, and seasonal median values ranging from 0.8 to 1.4m over the 2003-2009 period that are always larger than the corresponding modal values (0.6-1.1m) and lower than the mean values (1.0-1.6m), with standard deviation of 0.6-1.0m. An overall increasing trend of 0.03m/year of mean ice thickness is found from 2003 to 2009, although statistically insignificant (p=0.11) at the 95% confidence level. Starting from autumn, a general picture of seasonal mean, modal, and median ice thickness increases progressively from autumn to spring and decreases from spring to the following autumn, when new thin ice dominates the ice thickness distribution. The asymmetric shape of the thickness distribution reflects the key role of ice deformation processes in the evolution of the thickness distribution. The statistical properties of the thickness distribution interannually (high range of mean thickness and standard deviation) indicate the variability of deformation processes. However, spring ice volume, the product of ice mean thickness and areal extent computed for the spring maximum, shows variability year to year but is primarily dominated by ice extent variability, with no increasing or decreasing trend over this record length. The dependence of the volume on the ice extent primarily suggests that ice thickness changes have also not covaried with the ice extent losses seen over the satellite record in this region, unlike the Arctic. These properties reflect the interactive processes of ice advection, thermodynamic growth and ice deformation that all substantially influence ice mass balance in the Bellingshausen-Amundsen Seas region. C1 [Xie, Hongjie; Tekeli, Ahmet Emre; Ackley, Stephen F.] Univ Texas San Antonio, Dept Geol Sci, Lab Remote Sensing & Geoinformat, San Antonio, TX 78249 USA. [Tekeli, Ahmet Emre] King Saud Univ, Dept Civil Engn, Riyadh 11421, Saudi Arabia. [Yi, Donghui] NASA, Goddard Space Flight Ctr, SGT Inc, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Zwally, H. Jay] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. RP Xie, HJ (reprint author), Univ Texas San Antonio, Dept Geol Sci, Lab Remote Sensing & Geoinformat, San Antonio, TX 78249 USA. EM hongjie.xie@utsa.edu RI Xie, Hongjie/B-5845-2009 OI Xie, Hongjie/0000-0003-3516-1210 FU U.S. NASA [NNX08AQ87G]; NSF [AWT0703682] FX This research was supported by a U.S. NASA Grant (#NNX08AQ87G) and a NSF Grant (#AWT0703682). Provision of AMSR-E and NIC data from NASA and NOAA are greatly appreciated. We also want to thank Ling Du (Ocean University of China), Yunbo Bi (UTSA) and Anthony Arricale (UTSA) for help in processing some of the data, Nathan Kurtz (NASA/GSFC) for providing their data [Kurtz and Markus, 2012] for comparison, and the two anonymous reviewers and editor Andrey Proshutinsky for their constructive comments and suggestions that greatly improved the paper. We dedicate this paper in memory of our colleague and friend, Seymour Laxon, who pioneered in the application of satellite altimetry to the measurement of sea ice thickness. NR 48 TC 16 Z9 19 U1 2 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD MAY PY 2013 VL 118 IS 5 BP 2438 EP 2453 DI 10.1002/jgrc.20179 PG 16 WC Oceanography SC Oceanography GA 224TZ UT WOS:000324913700014 ER PT J AU Ofman, L Gedalin, M AF Ofman, L. Gedalin, M. TI Two-dimensional hybrid simulations of quasi-perpendicular collisionless shock dynamics: Gyrating downstream ion distributions SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Collisionless shocks; 2; 5D hybrid models; Ion velocity distributions ID MACH NUMBER SHOCKS; BOW SHOCK; MAGNETIC-FIELD; FRONT; NONSTATIONARITY; THERMALIZATION; STATIONARITY; WAVES; BETA AB Quasi-perpendicular collisionless shocks undergo structural changes with the increase of the Mach number. These changes are related to the increasing role of the reflected ions, which have a highly nongyrotropic distribution. Eventually, it is expected that the shock front becomes nonstationary. At low and moderate Mach numbers, the fraction of reflected ions is small, yet recent observations show the existence of a well-pronounced structure of the postshock magnetic field in the close vicinity of the transition layer. Large amplitude oscillations were earlier interpreted as waves generated by the shock front or passing through the shock in the downstream direction. Here we show, using two-dimensional hybrid simulations of quasi-perpendicular shocks, that the gyration of the directly transmitted ions downstream of the ramp produces the spatial pressure variations, which are accompanied with the observed magnetic oscillations due to the momentum conservation. In a wide range of the upstream ion temperatures, the low and moderate-Mach-number shocks remain stationary and one-dimensional, so that the magnetic and electric field depend only on the coordinate along the shock normal. The downstream ion distributions gradually gyrotropize due to the collisionless mixing of gyrophases. Nonstationary effects in these shocks do not affect noticeably the ion dynamics. However, we find that with the increase of the Mach number, shocks form rippled fronts in the low- and moderate- regimes. C1 [Ofman, L.] CUA, Greenbelt, MD USA. [Ofman, L.] NASA GSFC, Greenbelt, MD USA. [Gedalin, M.] Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel. RP Ofman, L (reprint author), CUA, Greenbelt, MD USA. EM Leon.Ofman@nasa.gov FU NASA [NNX10AC56G] FX LO would like to acknowledge discussions with A. F. Vinas, and support by NASA grant NNX10AC56G. NR 41 TC 10 Z9 10 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2013 VL 118 IS 5 BP 1828 EP 1836 DI 10.1029/2012JA018188 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800002 ER PT J AU Smith, EJ AF Smith, Edward J. TI Reply to comment by M. Lockwood and M. J. Owens on "What causes the flux excess in the heliospheric magnetic field?" SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Editorial Material DE heliospheric magnetic flux excess ID AU C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Smith, EJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Edward.J.Smith@jpl.nasa.gov NR 11 TC 1 Z9 1 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2013 VL 118 IS 5 BP 1888 EP 1890 DI 10.1002/jgra.50213 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800008 ER PT J AU Birn, J Hesse, M Nakamura, R Zaharia, S AF Birn, J. Hesse, M. Nakamura, R. Zaharia, S. TI Particle acceleration in dipolarization events SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE particle acceleration; injections; dipolarization ID TAIL CURRENT DISRUPTION; MODEL CURRENT SHEETS; ENERGETIC ELECTRONS; PLASMA SHEET; GEOSYNCHRONOUS OBSERVATIONS; MAGNETOSPHERIC SUBSTORMS; SPACECRAFT OBSERVATION; MAGNETIC RECONNECTION; SYNCHRONOUS ORBIT; FLUX TUBES AB Using the electromagnetic fields of a recent MHD simulation of magnetotail reconnection, flow bursts and dipolarization, we investigate the acceleration of test particles (protons and electrons) to suprathermal energies, confirming and extending earlier results on acceleration mechanisms and sources. (Part of the new results have been reviewed recently in Birn et al., Space Science Reviews, 167, doi:10.1007/ s11214-012-9874-4.) The test particle simulations reproduce major features of energetic particle events (injections) associated with substorms or other dipolarization events, particularly a rapid rise of energetic particle fluxes over limited ranges of energy. The major acceleration mechanisms for electrons are betatron acceleration and Fermi acceleration in the collapsing magnetic field. Ions, although non-adiabatic, undergo similar acceleration. Two major entry mechanisms into the acceleration site are identified: cross-tail drift from the inner tail plasma sheet and reconnection entry from field lines extending to the more distant plasma sheet. The former dominates early in an event and at higher energies (hundreds of keV) while the latter constitutes the main source later and at lower energies (tens of keV). Despite the fact that the injection front moves earthward in the tail, the peak of energetic particle fluxes moves to higher latitude when mapped from the near-Earth boundary to Earth in a static magnetic field model. C1 [Birn, J.] Space Sci Inst, Boulder, CO 80301 USA. [Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nakamura, R.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Zaharia, S.] Los Alamos Natl Lab, Los Alamos, NM USA. RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA. EM jbirn@spacescience.org RI Nakamura, Rumi/I-7712-2013; feggans, john/F-5370-2012; NASA MMS, Science Team/J-5393-2013 OI Nakamura, Rumi/0000-0002-2620-9211; NASA MMS, Science Team/0000-0002-9504-5214 FU U.S. Department of Energy; NASA [NNG08EJ63I, NNH111AQ42I]; NSF [1203711]; International Space Science Institute, Bern, Switzerland FX Most of this work was performed at Los Alamos under the auspices of the U.S. Department of Energy, supported by NASA grants NNG08EJ63I, NNH111AQ42I, and NSF grant 1203711. We are grateful to one of the referees for pointing out the relation between Fermi and betatron acceleration and the particle drifts. JB also thanks the International Space Science Institute, Bern, Switzerland, for hospitality and support. NR 69 TC 44 Z9 44 U1 3 U2 13 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 MAY PY 2013 VL 118 IS 5 BP 1960 EP 1971 DI 10.1002/jgra.50132 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800016 ER PT J AU Walsh, BM Ryou, AS Sibeck, DG Alexeev, II AF Walsh, B. M. Ryou, A. S. Sibeck, D. G. Alexeev, I. I. TI Energetic particle dynamics in Mercury's magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Mercury; energetic particles ID MESSENGER OBSERVATIONS; MAGNETIC-FIELD; ACCELERATION; EXOSPHERE; ELECTRONS; MODEL; TAIL; IONS AB We investigate the drift paths of energetic particles in Mercury's magnetosphere by tracing their motion through a model magnetic field. Test particle simulations solving the full Lorentz force show a quasi-trapped energetic particle population that gradient and curvature drift around the planet via Shabansky orbits, passing though high latitudes in the compressed dayside by equatorial latitudes on the nightside. Due to their large gyroradii, energetic H+ and Na+ ions will typically collide with the planet or the magnetopause and will not be able to complete a full drift orbit. These simulations provide direct comparison for recent spacecraft measurements from MESSENGER. Mercury's offset dipole results in an asymmetric loss cone and therefore an asymmetry in particle precipitation with more particles precipitating in the southern hemisphere. Since the planet lacks an atmosphere, precipitating particles will collide directly with the surface of the planet. The incident charged particles can kick up neutrals from the surface and have implications for the formation of the exosphere and weathering of the surface. C1 [Walsh, B. M.; Ryou, A. S.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ryou, A. S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Alexeev, I. I.] Moscow MV Lomonosov State Univ, Scobeltsyn Inst Nucl Phys, Moscow, Russia. RP Walsh, BM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM brian.m.walsh-1@nasa.gov RI Alexeev, Igor/G-8773-2011; Walsh, Brian/C-4899-2016 OI Walsh, Brian/0000-0001-7426-5413 FU National Science Foundation [AGS-1136827]; THEMIS project; RBSP project; Russian Foundation for Basic Research [11-05-00894, 12-02-92600-KO-a]; European FP7 project IMPEx [262863] FX Support was given by the National Science Foundation through grant AGS-1136827. A. S. Ryou and D. G. Sibeck were supported by the THEMIS and RBSP projects. I. I. Alexeev was supported by the Russian Foundation for Basic Research grants 11-05-00894 and 12-02-92600-KO-a, and the European FP7 project IMPEx (262863). The authors would also like to thank A. Glocer, T. Sundberg, and C. Schmidt for useful discussions. Masaki Fujimoto thanks the reviewers for their assistance in evaluating this paper. NR 40 TC 3 Z9 3 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2013 VL 118 IS 5 BP 1992 EP 1999 DI 10.1002/jgra.50266 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800019 ER PT J AU McGrath, MA Jia, XZ Retherford, K Feldman, PD Strobel, DF Saur, J AF McGrath, Melissa A. Jia, Xianzhe Retherford, Kurt Feldman, Paul D. Strobel, Darrell F. Saur, Joachim TI Aurora on Ganymede SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ganymede ID MAGNETIC-FIELD; GALILEAN SATELLITES; MAGNETOSPHERE; SIMULATIONS; SPACECRAFT; ELECTRONS AB We present four sets of ultraviolet images of Ganymede acquired with the Hubble Space Telescope (HST) from 1998 to 2007, all of which show auroral emission from electron excited atomic oxygen. The three different hemispheres of Ganymede captured in the observations show strikingly different emission morphologies. Ultraviolet emission at 1356 angstrom is brightest at relatively high latitude on the orbital trailing (upstream plasma) hemisphere and in an auroral oval that extends to as low as similar to 10 degrees N latitude on the orbital leading (downstream plasma) hemisphere. Two sets of images of the Jupiter-facing hemisphere acquired at nearly the same sub-Earth longitude but separated by similar to 4 years show very similar emission morphology that is consistent with the pattern of emission seen in the upstream and downstream images: the emission is at high latitude in the upstream quadrant and at low latitude in the downstream quadrant. This implies that the large-scale, nominal auroral oval on Ganymede is apparently quite stable with time, despite significant brightness fluctuations within the overall stable pattern during the 10-30min time scale between individual images. The overall emission morphology appears to be driven primarily by the strong Jovian magnetospheric plasma interaction with Ganymede and does not appear to be strongly influenced by the orientation of the background Jovian magnetic field. The observed auroral oval pattern is reasonably well matched by a magnetohydrodymanic (MHD) model optimized to fit the Galileo magnetic field measurements near Ganymede. The location of the auroral oval from these data provides a reasonable match to the location of the well-defined visible boundary of the Ganymede polar cap except in the northern, leading hemisphere. C1 [McGrath, Melissa A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Jia, Xianzhe] Univ Michigan, Ann Arbor, MI 48109 USA. [Retherford, Kurt] Southwest Res Inst, San Antonio, TX USA. [Feldman, Paul D.; Strobel, Darrell F.] Johns Hopkins Univ, Baltimore, MD USA. [Saur, Joachim] Univ Cologne, D-50931 Cologne, Germany. RP McGrath, MA (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM melissa.a.mcgrath@nasa.gov RI Jia, Xianzhe/C-5171-2012; OI Jia, Xianzhe/0000-0002-8685-1484; Retherford, Kurt/0000-0001-9470-150X FU NASA [NAS 5-26555]; NASA through Space Telescope Science Institute FX This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 7939, 8224, 9296, and 10871. Support for program 8224 to MMcG, PDF, and DFS was provided by NASA through a grant from the Space Telescope Science Institute. We thank N. Murphy and R. Pappalardo for providing the Galileo image shown in Figure 8 and K. Khurana for providing previously published results in digital format. NR 28 TC 18 Z9 18 U1 0 U2 7 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 MAY PY 2013 VL 118 IS 5 BP 2043 EP 2054 DI 10.1002/jgra.50122 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800023 ER PT J AU Wang, Y Sibeck, DG Merka, J Boardsen, SA Karimabadi, H Sipes, TB Safrankova, J Jelinek, K Lin, R AF Wang, Y. Sibeck, D. G. Merka, J. Boardsen, S. A. Karimabadi, H. Sipes, T. B. Safrankova, J. Jelinek, K. Lin, R. TI A new three-dimensional magnetopause model with a support vector regression machine and a large database of multiple spacecraft observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetopause; empirical model; support vector regression machine; dipole tilt; erosion ID SOLAR-WIND CONTROL; MAGNETIC-FIELD; GEOMAGNETIC FIELD; EMPIRICAL-MODEL; SHAPE; PRESSURE; SIZE; LOCATION; AVERAGE AB We present results from a new three-dimensional empirical magnetopause model based on 15,089 magnetopause crossings from 23 spacecraft. To construct the model, we introduce a Support Vector Regression Machine (SVRM) technique with a systematic approach that balances model smoothness with fitting accuracy to produce a model that reveals the manner in which the size and shape of the magnetopause depend upon various control parameters without any assumptions concerning the analytical shape of the magnetopause. The new model fits the data used in the modeling very accurately, and can guarantee a similar accuracy when predicting unseen observations within the applicable range of control parameters. We introduce a new error analysis technique based upon the SVRM that enables us to obtain model errors appropriate to different locations and control parameters. We find significant east-west elongations in the magnetopause shape for many combinations of control parameters. Variations in the Earth's dipole tilt can cause significant magnetopause north/south asymmetries and deviation of the magnetopause nose from the Sun-Earth line nonlinearly by as much as 5Re. Subsolar magnetopause erosion effect under southward IMF is seen which is strongly affected by solar wind dynamic pressure. Further, we find significant shrinking of high-latitude magnetopause with decreased magnetopause flaring angle during northward IMF. C1 [Wang, Y.; Sibeck, D. G.; Merka, J.; Boardsen, S. A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Wang, Y.; Merka, J.; Boardsen, S. A.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA. [Karimabadi, H.; Sipes, T. B.] SciberQuest Inc, Del Mar, CA USA. [Safrankova, J.; Jelinek, K.] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic. [Lin, R.] Chinese Acad Sci, Natl Space Sci Ctr, Beijing, Peoples R China. RP Wang, Y (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Mail Stop 674, Greenbelt, MD 20771 USA. EM yongli.wang@nasa.gov FU NASA Geospace SRT Program [NNX09AP16G]; NASA's Heliophysics Data Environment Enhancements Program FX We thank both reviewers for their valuable comments and constructive suggestions. The work at GSFC was supported by NASA Geospace SR&T Program under grant NNX09AP16G. Work at SciberQuest, Inc. was supported by NASA's Heliophysics Data Environment Enhancements Program. We thank the Cluster FGM, CIS, and PEACE instrument teams and ESA Cluster Active Archive for Cluster data. We thank Space Physics Data Facility (SPDF) and National Space Science Data Center (NSSDC) for providing the OMNI data set. NR 30 TC 9 Z9 9 U1 2 U2 9 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 MAY PY 2013 VL 118 IS 5 BP 2173 EP 2184 DI 10.1002/jgra.50226 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800033 ER PT J AU Winslow, RM Anderson, BJ Johnson, CL Slavin, JA Korth, H Purucker, ME Baker, DN Solomon, SC AF Winslow, Reka M. Anderson, Brian J. Johnson, Catherine L. Slavin, James A. Korth, Haje Purucker, Michael E. Baker, Daniel N. Solomon, Sean C. TI Mercury's magnetopause and bow shock from MESSENGER Magnetometer observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE magnetopause; bow shock; Mercury; MESSENGER Magnetometer; Mercury's magnetosphere ID SOLAR-WIND CONTROL; MAGNETIC-FIELD; TERRESTRIAL PLANETS; MACH NUMBERS; SHAPE; MAGNETOSPHERE; MODEL; LOCATIONS; POSITION; FLOW AB We have established the average shape and location of Mercury's magnetopause and bow shock from orbital observations by the MESSENGER Magnetometer. We fit empirical models to midpoints of boundary crossings and probability density maps of the magnetopause and bow shock positions. The magnetopause was fit by a surface for which the position R from the planetary dipole varies as [1+cos()](-), where is the angle between R and the dipole-Sun line, the subsolar standoff distance R-ss is 1.45 R-M (where R-M is Mercury's radius), and the flaring parameter =0.5. The average magnetopause shape and location were determined under a mean solar wind ram pressure P-Ram of 14.3 nPa. The best fit bow shock shape established under an average Alfven Mach number (M-A) of 6.6 is described by a hyperboloid having R-ss=1.96 R-M and an eccentricity of 1.02. These boundaries move as P-Ram and M-A vary, but their shapes remain unchanged. The magnetopause R-ss varies from 1.55 to 1.35 R-M for P-Ram in the range of 8.8-21.6 nPa. The bow shock R-ss varies from 2.29 to 1.89 R-M for M-A in the range of 4.12-11.8. The boundaries are well approximated by figures of revolution. Additional quantifiable effects of the interplanetary magnetic field are masked by the large dynamic variability of these boundaries. The magnetotail surface is nearly cylindrical, with a radius of similar to 2.7 R-M at a distance of 3 R-M downstream of Mercury. By comparison, Earth's magnetotail flaring continues until a downstream distance of similar to 10 R-ss. C1 [Winslow, Reka M.; Johnson, Catherine L.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z1, Canada. [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ USA. [Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Purucker, Michael E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Winslow, RM (reprint author), Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z1, Canada. EM rwinslow@eos.ubc.ca RI Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA [NAS5-97271, NASW-00002]; MESSENGER [NNX11AB84G, NNH08CC05C]; Natural Sciences and Engineering Research Council of Canada FX The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. C. L. J. and M. E. P. are supported by MESSENGER Participating Scientist grants NNX11AB84G and NNH08CC05C. R. M. W. and C. L. J. acknowledge support from the Natural Sciences and Engineering Research Council of Canada. We thank the Community Coordinated Modeling Center for providing ENLIL model runs. The authors thank the reviewers for constructive comments. NR 59 TC 44 Z9 44 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2013 VL 118 IS 5 BP 2213 EP 2227 DI 10.1002/jgra.50237 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800036 ER PT J AU Mitchell, EJ Fok, MCH Lopez, RE Lyon, JG AF Mitchell, Elizabeth J. Fok, Mei-Ching H. Lopez, Ramon E. Lyon, John G. TI Simulated ring current response during periods of dawn-dusk oriented interplanetary magnetic field (B-y) SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE Dawn-dusk IMF; Ring Current; LFM MHD; CRCM; Flank reconnection ID TRANSPOLAR POTENTIAL SATURATION; ART. NO. A09203; MHD SIMULATIONS; MAGNETOSPHERE; MODEL; DECAY; CONVECTION; IONS AB Ring current formation is mainly attributed to enhanced global magnetospheric convection and particle injection. One of the indicators of enhanced global magnetospheric convection is the transpolar potential. The transpolar potential has been shown to respond to dawn-dusk oriented interplanetary magnetic field (IMF), enhancing as the IMF magnitude grows. This suggests that the ring current should respond to dawn-dusk oriented IMF. This work examines the ring current response during periods of dawn-dusk oriented IMF using the Lyon-Fedder-Mobarry and Comprehensive Ring Current Model simulations. Exploring three hypotheses, this work shows through simulation results that the ring current does respond during periods of dawn-dusk oriented IMF, that the inner magnetospheric response is different for periods of dawn-dusk oriented IMF than for periods of southward IMF, and that these differences are attributed to both lower magnetospheric convection on closed field lines and the location of the reconnection region on the nightside. Specifically, the simulation results show that as the magnitude of the dawn-dusk oriented IMF increases, producing a corresponding increase in the transpolar potential, the ring current response increases. The response is always much less than a comparable southward IMF would produce. This lower response is due to both magnetospheric convection on closed field lines, which builds the ring current but at a slower rate, and flank reconnection, which allows energy to flow through the inner magnetosphere without building the ring current plasma population (as a conduit). C1 [Mitchell, Elizabeth J.] NASA, Goddard Space Flight Ctr, ORAU, Greenbelt, MD 20771 USA. [Fok, Mei-Ching H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lopez, Ramon E.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Lyon, John G.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. Dept Phys & Astron, Dartmouth Coll, Hanover, NH USA. RP Mitchell, EJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd,200-W254, Laurel, MD 20723 USA. EM Elizabeth.Mitchell@jhuapl.edu RI Fok, Mei-Ching/D-1626-2012; Mitchell, Elizabeth /E-6156-2017; OI Mitchell, Elizabeth /0000-0001-5014-9493; Lopez, Ramon/0000-0001-5881-1365 FU NASA [4200254162ESAX22008D, NNX09AI63G]; NSF [ATM-0900920]; CISM; STC Program of the National Science Foundation [ATM-0120950] FX This material is based upon work supported by the NASA Postdoctoral Program as well as work supported by NASA grant 4200254162ESAX22008D, NASA grant NNX09AI63G, NSF grant ATM-0900920, and CISM (which is funded by the STC Program of the National Science Foundation under agreement ATM-0120950). NR 35 TC 1 Z9 1 U1 0 U2 2 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 MAY PY 2013 VL 118 IS 5 BP 2228 EP 2243 DI 10.1002/jgra.50269 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800037 ER PT J AU Tsurutani, BT Lakhina, GS Verkhoglyadova, OP AF Tsurutani, Bruce T. Lakhina, Gurbax S. Verkhoglyadova, Olga P. TI Energetic electron (> 10 keV) microburst precipitation, similar to 5-15 s X-ray pulsations, chorus, and wave-particle interactions: A review SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE microbursts; microburst trains; electron pulsations; chorus; chorus elements; mirror modes ID LOW-FREQUENCY EMISSIONS; OUTER RADIATION BELT; WHISTLER-MODE CHORUS; STORM-TIME CHORUS; AURORAL-ZONE; LION ROARS; BALLOON OBSERVATIONS; ROCKET OBSERVATIONS; MAGNETIC STORMS; ELF/VLF CHORUS AB The fundamental features of similar to 0.1-0.2s duration similar to 0.5s spaced ionospheric electron precipitation microbursts, similar to 5 to 15s microburst trains, and 5-15s electron precipitation pulsations are reviewed in light of similar temporal structures of electromagnetic whistler mode chorus waves detected in the outer magnetosphere. Past observations of microbursts point to extremely rapid (ms timescale) wave-particle interactions, probably between lower band chorus subelements (durations of similar to 10 to 100ms) and energetic similar to 10 to 100keV electrons. A recent theory explaining such rapid interaction rates observed in microbursts is briefly reviewed. Arguments are given why similar to 5-15s X-ray (and optical) pulsations are also associated with chorus scattering of energetic electrons. Comments about relativistic (E>1MeV) microbursts are also provided. There are, however, many other unsolved problems of outer zone energetic electron precipitation. The authors will attempt to indicate several of these for the interested reader. Finally, an appendix is provided for a brief review of two-frequency chorus and some current problems with that topic. C1 [Tsurutani, Bruce T.; Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lakhina, Gurbax S.] Indian Inst Geomagnetism, Navi Mumbai, India. RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bruce.tsurutani@jpl.nasa.gov FU Indian National Science Academy, New Delhi FX This work is dedicated to the late Kinsey A. Anderson, who with his coworkers and former students did much to advance our understanding of microburst physics. Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. B. T. T. thanks P. Bellan and Cal. Tech. for hosting him during a sabbatical leave. G. S. L. thanks the Indian National Science Academy, New Delhi, for support under the Senior Scientist Scheme. NR 104 TC 25 Z9 25 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY PY 2013 VL 118 IS 5 BP 2296 EP 2312 DI 10.1002/jgra.50264 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800041 ER PT J AU Connaughton, V Briggs, MS Xiong, SL Dwyer, JR Hutchins, ML Grove, JE Chekhtman, A Tierney, D Fitzpatrick, G Foley, S McBreen, S Bhat, PN Chaplin, VL Cramer, E Fishman, GJ Holzworth, RH Gibby, M von Kienlin, A Meegan, CA Paciesas, WS Preece, RD Wilson-Hodge, C AF Connaughton, Valerie Briggs, Michael S. Xiong, Shaolin Dwyer, Joseph R. Hutchins, Michael L. Grove, J. Eric Chekhtman, Alexandre Tierney, Dave Fitzpatrick, Gerard Foley, Suzanne McBreen, Shelia Bhat, P. N. Chaplin, Vandiver L. Cramer, Eric Fishman, Gerald J. Holzworth, Robert H. Gibby, Melissa von Kienlin, Andreas Meegan, Charles A. Paciesas, William S. Preece, Robert D. Wilson-Hodge, Colleen TI Radio signals from electron beams in terrestrial gamma ray flashes SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE gamma-ray; lightning; radio; Fermi GBM; WWLLN ID LIGHTNING LOCATION NETWORK AB We show that the rate of association between terrestrial gamma ray flashes (TGFs) observed by the Fermi gamma ray burst monitor and VLF discharges detected by the World Wide Lightning Location Network (WWLLN) depends strongly on the duration of the TGF, with the shortest TGFs having associated WWLLN events over 50% of the time, and the longest TGFs showing a less than 10% match rate. This correlation is stronger if one excludes the WWLLN discharges that are not simultaneous (within 200 mu s) with the TGF. We infer that the simultaneous VLF discharges are from the relativistic electron avalanches that are responsible for the flash of gamma rays and the nonsimultaneous VLF discharges are from related intracloud lightning strokes. The distributions of far-field radiated VLF stroke energy measured by WWLLN for the simultaneous and nonsimultaneous discharges support the hypothesis of two discrete populations of VLF signals associated with TGFs, with the simultaneous discharges among the strongest measured by WWLLN. C1 [Connaughton, Valerie; Briggs, Michael S.; Xiong, Shaolin; Bhat, P. N.; Chaplin, Vandiver L.; Preece, Robert D.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Connaughton, Valerie; Briggs, Michael S.; Preece, Robert D.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Dwyer, Joseph R.; Cramer, Eric] Florida Inst Technol, Melbourne, FL 32901 USA. [Hutchins, Michael L.; Holzworth, Robert H.] Univ Washington, Seattle, WA 98195 USA. [Grove, J. Eric] US Naval Res Lab, Space Sci Div, Washington, DC USA. [Chekhtman, Alexandre] George Mason Univ, Fairfax, VA 22030 USA. [Tierney, Dave; Fitzpatrick, Gerard; Foley, Suzanne; McBreen, Shelia] Univ Coll Dublin, Dublin 4, Ireland. [Fishman, Gerald J.; Gibby, Melissa] Jacobs Engn Grp Inc, Huntsville, AL USA. [von Kienlin, Andreas] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Meegan, Charles A.; Paciesas, William S.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Wilson-Hodge, Colleen] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Connaughton, V (reprint author), Univ Alabama, CSPAR, Huntsville, AL 35899 USA. EM connauv@uah.edu OI Preece, Robert/0000-0003-1626-7335 FU National Aeronautics and Space Administration (NASA) in the United States; Bundesministerium fur Wirtschaft und Technologie (BMWi) / Deutsches Zentrum fur Luft und Raumfahrt (DLR) in Germany; NASA's Fermi Guest Investigator Program; DARPA [HR0011-10-1-0061]; Science Foundation Ireland [09-RFP-AST-2400]; Irish Research Council for Science, Engineering and Technology; Marie Curie Actions under FP7 FX The Fermi GBM Collaboration acknowledges support for GBM development, operations, and data analysis from National Aeronautics and Space Administration (NASA) in the United States and from the Bundesministerium fur Wirtschaft und Technologie (BMWi) / Deutsches Zentrum fur Luft und Raumfahrt (DLR) in Germany. This work was supported in part by NASA's Fermi Guest Investigator Program and by DARPA grant HR0011-10-1-0061. D. T. acknowledges support from Science Foundation Ireland under grant number 09-RFP-AST-2400. S. F. and G. F. acknowledge the support of the Irish Research Council for Science, Engineering and Technology; S. F. is cofunded by Marie Curie Actions under FP7. The authors wish to thank the World Wide Lightning Location Network (http://wwlln.net), a collaboration among over 50 universities and institutions, for providing the lightning location data used in this paper. We appreciate the freely-available Coyote resources for IDL programming, which helped generate all the histograms in this paper (http://www.idlcoyote.com/). We thank Nikolai Ostgaard and an anonymous reviewer for helpful suggestions during the refereeing process. NR 40 TC 24 Z9 24 U1 1 U2 10 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 MAY PY 2013 VL 118 IS 5 BP 2313 EP 2320 DI 10.1029/2012JA018288 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800042 ER PT J AU Dao, E Kelley, MC Pfaff, RF Roddy, PA AF Dao, E. Kelley, M. C. Pfaff, R. F. Roddy, P. A. TI Large-scale structures in the equatorial ionosphere and their connection to the generalized Rayleigh-Taylor instability SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE irregularities; space weather; scintillations; equatorial electric fields; large scale convective storms ID F-REGION; SPREAD-F AB For the first time, electric field and density fluctuations have been simultaneously measured on the Communications/Navigation Outage Forecasting System satellite at large scales (>300km). The ratio of their spectral power rises as k(2), unlike scales from 20m to 300km where the ratio is independent of k. We suggest that gravity waves dominate these large scales and mix with density gradients via self-generated electric fields to form n/n(0). C1 [Dao, E.; Kelley, M. C.] Cornell Univ, Sch Elect & Comp Engn, Ithaca, NY 14853 USA. [Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. [Roddy, P. A.] Air Force Res Lab, Space Vehicles Directorate, Hanscom AFB, MA USA. RP Kelley, MC (reprint author), Cornell Univ, Sch Elect & Comp Engn, Ithaca, NY 14853 USA. EM mck13@cornell.edu FU Air Force Research Laboratory; Department of Defense Space Test Program; National Aeronautics and Space Administration; Naval Research Laboratory; Aerospace Corporation; NASA [NNH09AK05I, NNH09AM20I]; Office of Naval Research [N00014-09-1-0975]; National Science Foundation [ATM-0551107] FX The C/NOFS mission is supported by the Air Force Research Laboratory, the Department of Defense Space Test Program, the National Aeronautics and Space Administration, the Naval Research Laboratory, and the Aerospace Corporation. The analysis was supported in part by NASA grant NNH09AK05I and NNH09AM20I to the Air Force Research Laboratory. Work at Cornell was funded by the Office of Naval Research under grant N00014-09-1-0975 and by the National Science Foundation under grant ATM-0551107. NR 14 TC 0 Z9 0 U1 2 U2 3 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 MAY PY 2013 VL 118 IS 5 BP 2618 EP 2622 DI 10.1002/jgra.50283 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800068 ER PT J AU Haaser, RA Davidson, R Heelis, RA Earle, GD Venkatraman, S Klenzing, J AF Haaser, R. A. Davidson, R. Heelis, R. A. Earle, G. D. Venkatraman, S. Klenzing, J. TI Storm time meridional wind perturbations in the equatorial upper thermosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE solar; Geomagnetic; storm; thermosphere; CNOFS; ionosphere ID NEUTRAL WINDS; IMAGING INTERFEROMETER; GEOMAGNETIC STORMS; UPPER-ATMOSPHERE; IONOSPHERE; SATELLITE; TEMPERATURES; LATITUDE; DENSITY; PERIOD AB We present observations from the Coupled Ion Neutral Dynamics Investigation (CINDI) of storm time meridional winds in the neutral atmosphere near the magnetic equator at 400km altitude. Observations near the magnetic equator in the southern geographic hemisphere are dominated by energy inputs from the southern Polar Regions that produce south to north (equatorward) wind perturbations to accompany perturbations in the neutral density and temperature. In one exceptional case, when observations are made near midnight and the north magnetic pole rotates through the midnight sector, north to south (poleward) meridional wind perturbations are observed just south of the magnetic equator. Accompanying perturbations in the neutral density on the dayside and the nightside are consistent with observed increases in the ion temperature and inferred increases in the neutral temperature in accord with hydrostatic equilibrium. C1 [Haaser, R. A.; Heelis, R. A.; Venkatraman, S.] Univ Texas Dallas, William B Hanson Ctr Space Sci, Richardson, TX 75080 USA. [Davidson, R.; Earle, G. D.] Virginia Tech, Ctr Space Sci & Engn, Blacksburg, VA USA. [Klenzing, J.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Haaser, RA (reprint author), Univ Texas Dallas, William B Hanson Ctr Space Sci, 800 W Campbell Rd,WT 15, Richardson, TX 75080 USA. EM rhaaser@utdallas.edu RI Klenzing, Jeff/E-2406-2011 OI Klenzing, Jeff/0000-0001-8321-6074 FU NASA [NNX10AT02G] FX This work is supported by NASA grant NNX10AT02G to the University of Texas at Dallas. NR 30 TC 3 Z9 3 U1 0 U2 5 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 MAY PY 2013 VL 118 IS 5 BP 2756 EP 2764 DI 10.1002/jgra.50299 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228UF UT WOS:000325215800080 ER PT J AU Greene, CH Meyer-Gutbrod, E Monger, BC McGarry, LP Pershing, AJ Belkin, IM Fratantoni, PS Mountain, DG Pickart, RS Proshutinsky, A Ji, RB Bisagni, JJ Hakkinen, SMA Haidvogel, DB Wang, J Head, E Smith, P Reid, PC Conversi, A AF Greene, Charles H. Meyer-Gutbrod, Erin Monger, Bruce C. McGarry, Louise P. Pershing, Andrew J. Belkin, Igor M. Fratantoni, Paula S. Mountain, David G. Pickart, Robert S. Proshutinsky, Andrey Ji, Rubao Bisagni, James J. Hakkinen, Sirpa M. A. Haidvogel, Dale B. Wang, Jia Head, Erica Smith, Peter Reid, Philip C. Conversi, Alessandra TI Remote climate forcing of decadal-scale regime shifts in Northwest Atlantic shelf ecosystems SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID CALANUS-FINMARCHICUS POPULATIONS; COD GADUS-MORHUA; GULF-OF-MAINE; INTERANNUAL VARIABILITY; MARINE ECOSYSTEMS; ARCTIC CLIMATE; SCOTIAN SHELF; RIGHT WHALES; BARENTS SEA; OSCILLATION AB Decadal-scale regime shifts in Northwest Atlantic shelf ecosystems can be remotely forced by climate-associated atmosphere-ocean interactions in the North Atlantic and Arctic Ocean Basins. This remote climate forcing is mediated primarily by basin- and hemispheric-scale changes in ocean circulation. We review and synthesize results from process-oriented field studies and retrospective analyses of time-series data to document the linkages between climate, ocean circulation, and ecosystem dynamics. Bottom-up forcing associated with climate plays a prominent role in the dynamics of these ecosystems, comparable in importance to that of top-down forcing associated with commercial fishing. A broad perspective, one encompassing the effects of basin-and hemispheric-scale climate processes on marine ecosystems, will be critical to the sustainable management of marine living resources in the Northwest Atlantic. C1 [Greene, Charles H.; Meyer-Gutbrod, Erin; Monger, Bruce C.; McGarry, Louise P.] Cornell Univ, Ocean Resources & Ecosyst Program, Ithaca, NY 14853 USA. [Meyer-Gutbrod, Erin] Gulf Maine Res Inst, Portland, ME USA. [Pershing, Andrew J.] Univ Maine, Sch Marine Sci, Orono, ME USA. [Belkin, Igor M.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. [Fratantoni, Paula S.] NOAA, Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, Woods Hole, MA 02543 USA. [Pickart, Robert S.; Proshutinsky, Andrey] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA. [Ji, Rubao] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. [Bisagni, James J.] Univ Massachusetts Dartmouth, Sch Marine Sci & Technol, New Bedford, MA USA. [Hakkinen, Sirpa M. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Haidvogel, Dale B.] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA. [Wang, Jia] NOAA, Great Lakes Environm Res Lab, Ann Arbor, MI 48105 USA. [Head, Erica; Smith, Peter] Bedford Inst Oceanog, Dept Fisheries & Oceans, Dartmouth, NS, Canada. [Reid, Philip C.; Conversi, Alessandra] Sir Alister Hardy Fdn Ocean Sci, Plymouth, Devon, England. [Conversi, Alessandra] Italian Natl Res Council, Inst Marine Sci, La Spezia, Italy. [Conversi, Alessandra] Univ Plymouth, Inst Marine, Plymouth PL4 8AA, Devon, England. RP Greene, CH (reprint author), Cornell Univ, Ocean Resources & Ecosyst Program, Ithaca, NY 14853 USA. EM chg2@cornell.edu RI CNR, Ismar/P-1247-2014; Ji, Rubao/I-1970-2015; Conversi, Alessandra/G-3899-2011 OI CNR, Ismar/0000-0001-5351-1486; Ji, Rubao/0000-0002-8839-5427; Conversi, Alessandra/0000-0002-8566-8282 FU National Science Foundation, Regional and Pan-Regional Synthesis Phases of the U.S. Global Ocean Ecosystem (GLOBEC) Program FX We thank the Gulf of Maine Research Institute, Cornell University's Shoals Marine Laboratory, and the University of Washington's Friday Harbor Laboratories (FHL) for hosting the research workshops at which the ideas in this paper were developed. C.H.G. thanks FHL for hosting him as a Whiteley Center Scholar during the preparation of this manuscript. Funding for this research was provided by the National Science Foundation as part of the Regional and Pan-Regional Synthesis Phases of the U.S. Global Ocean Ecosystem (GLOBEC) Program. NR 105 TC 21 Z9 21 U1 6 U2 46 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-3590 EI 1939-5590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD MAY PY 2013 VL 58 IS 3 BP 803 EP 816 DI 10.4319/lo.2013.58.3.0803 PG 14 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 192NG UT WOS:000322491100004 ER PT J AU Besserer, J Nimmo, F Roberts, JH Pappalardo, RT AF Besserer, J. Nimmo, F. Roberts, J. H. Pappalardo, R. T. TI Convection-driven compaction as a possible origin of Enceladus's long wavelength topography SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Enceladus; topography; porosity; convection ID SOUTH-POLE; EPISODIC VOLCANISM; INTERNAL STRUCTURE; PHASE-TRANSITION; ICY SATELLITES; COMET NUCLEI; HEAT; CONSEQUENCES; EVOLUTION; RESERVOIR AB The long wavelength surface topography of Enceladus shows depressions about 1 km in depth and approximate to 10(2)km wide. One possible cause of this topography is spatially variable amounts of compaction of an initially porous ice shell, driven by spatial variations in heat flux. Here, we show that the heat flux variations associated with convection in the shell can quantitatively match the observed features. We develop a simple model of viscous compaction that includes the effect of porosity on thermal conductivity, and find that an initial shell porosity of at least 20-25% is required to develop the observed topography over approximate to 1 Ga. This mechanism produces topographic depressions, not rises, above convective upwellings, and does not generate detectable gravity anomalies. Unlike transient dynamic topography, it can potentially leave a permanent record of ancient convective processes in the shallow lithospheres of icy satellites. C1 [Besserer, J.; Nimmo, F.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Roberts, J. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Pappalardo, R. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Besserer, J (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA. EM jbessere@ucsc.edu RI Roberts, James/I-9030-2012 FU NASA [NNX11AK44G, NAS2-03144, NNX12AK44G]; CDAPS program FX This research is supported by NASA grants NNX11AK44G, NAS2-03144 and the CDAPS program to FN, and NASA grant NNX12AK44G to JHR. The portion of this work performed by RTP was performed under a contract with the NASA. The authors thank the editor, M.A. Wieczorek, and two anonymous reviewers for their comments that helped improve the manuscript. NR 45 TC 15 Z9 15 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY PY 2013 VL 118 IS 5 BP 908 EP 915 DI 10.1002/jgre.20079 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400003 ER PT J AU Siegler, MA Bills, BG Paige, DA AF Siegler, Matthew A. Bills, Bruce G. Paige, D. A. TI Orbital eccentricity driven temperature variation at Mercury's poles SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mercury; eccentricity; temperature; ice; polar; thermal ID PLANET MERCURY; SOLAR-SYSTEM; THERMAL-STABILITY; POLAR ANOMALIES; ICE; OBLIQUITY; EVOLUTION; DEPOSITS; ROTATION; CHAOS AB Due to Mercury's extremely small obliquity, variations in orbital eccentricity are likely to have been the dominant cause of changes in polar temperatures on Mercury throughout the bulk of its history. In the last 10Myr, the eccentricity has varied between 0.1 and 0.3. Over the past 100Myr, eccentricity extremes of nearly zero to greater than 0.4 have likely been reached. We calculate the temperature in the near-polar region (within 10 degrees of the North Pole) as it varies in response to past eccentricities. These calculations show periods with dramatically different temperatures, diurnal amplitudes, and long period thermal cyclesall of which can have a dramatic effect on longitudinal variations in long-term subsurface ice stability. Given forthcoming topographic data, thermal models including long-term eccentricity can help constrain when past ice might have been delivered to Mercury. C1 [Siegler, Matthew A.; Bills, Bruce G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Siegler, Matthew A.; Paige, D. A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. RP Siegler, MA (reprint author), Univ Calif Los Angeles, Jet Prop Lab, Los Angeles, CA 90095 USA. EM matthew.a.siegler@jpl.nasa.gov FU National Aeronautics and Space Administration FX Thank you to Jean-Luc Margot, David Jewitt, Dana Hurley, Ashwin Vasavada, and Jean-Pierre Williams for useful discussions. Thank you to Sue Smrekar for the patience as I finished another fraction of my thesis. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. (c) 2012. All rights reserved. NR 50 TC 6 Z9 6 U1 1 U2 5 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 MAY PY 2013 VL 118 IS 5 BP 930 EP 937 DI 10.1002/jgre.20070 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400005 ER PT J AU Potter, RWK Kring, DA Collins, GS Kiefer, WS McGovern, PJ AF Potter, Ross W. K. Kring, David A. Collins, Gareth S. Kiefer, Walter S. McGovern, Patrick J. TI Numerical modeling of the formation and structure of the Orientale impact basin SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE impact basins; basin formation; lunar cataclysm; late heavy bombardment; Orientale; Chicxulub ID PEAK-RING FORMATION; CHICXULUB CRATER; HYDROCODE SIMULATIONS; MANTLE CONVECTION; OBLIQUE IMPACTS; MELT PRODUCTION; LUNAR BASINS; MOON; ORIGIN; TARGETS AB The Orientale impact basin is the youngest and best-preserved lunar multi-ring basin and has, thus, been the focus of studies investigating basin-forming processes and final structures. A consensus about how multi-ring basins form, however, remains elusive. Here we numerically model the Orientale basin-forming impact with the aim of resolving some of the uncertainties associated with this basin. By using two thermal profiles estimating lunar conditions at the time of Orientale's formation and constraining the numerical models with crustal structures inferred from gravity data, we provide estimates for Orientale's impact energy (2-9 x10(25)J), impactor size (50-80km diameter), transient crater size (approximate to 320-480km), excavation depth (40-55km), and impact melt volume (approximate to 10(6)km(3)). We also analyze the distribution and deformation of target material and compare our model results and Orientale observations with the Chicxulub crater to investigate similarities between these two impact structures. C1 [Potter, Ross W. K.; Kring, David A.; Kiefer, Walter S.; McGovern, Patrick J.] Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA. [Potter, Ross W. K.; Kring, David A.; Kiefer, Walter S.; McGovern, Patrick J.] NASA, Lunar Sci Inst, Moffett Field, CA USA. [Collins, Gareth S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. RP Potter, RWK (reprint author), Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM potter@lpi.usra.edu OI McGovern, Patrick/0000-0001-9647-3096; Collins, Gareth/0000-0002-6087-6149; Kiefer, Walter/0000-0001-6741-5460 FU NASA Lunar Science Institute [NNA09DB33A]; STFC [ST/J001260/1]; NERC [NE/E013589/1] FX We thank Boris Ivanov, Jay Melosh, Kai Wunnemann and Dirk Elbeshausen for their work developing iSALE. This work was partially supported by NASA Lunar Science Institute contract NNA09DB33A (PI David A. Kring). We also acknowledge STFC grant ST/J001260/1 and NERC grant NE/E013589/1. The authors thank Boris Ivanov and an anonymous reviewer for their constructive, and overall positive, reviews of this paper. NR 87 TC 23 Z9 23 U1 0 U2 5 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 MAY PY 2013 VL 118 IS 5 BP 963 EP 979 DI 10.1002/jgre.20080 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400008 ER PT J AU Guzewich, SD Toigo, AD Richardson, MI Newman, CE Talaat, ER Waugh, DW McConnochie, TH AF Guzewich, Scott D. Toigo, Anthony D. Richardson, Mark I. Newman, Claire E. Talaat, Elsayed R. Waugh, Darryn W. McConnochie, Timothy H. TI The impact of a realistic vertical dust distribution on the simulation of the Martian General Circulation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars Atmosphere; Dust; GCM Modeling ID STATIONARY PLANETARY-WAVES; THERMAL TIDES; MIDDLE ATMOSPHERE; MODEL SIMULATION; DIURNAL TIDE; MARS SURFACE; 15-MU-M BAND; STORMS; CYCLE; WINTER AB Limb-scanning observations with the Mars Climate Sounder and Thermal Emission Spectrometer (TES) have identified discrete layers of enhanced dust opacity well above the boundary layer and a mean vertical structure of dust opacity very different from the expectation of well-mixed dust in the lowest 1-2 scale heights. To assess the impact of this vertical dust opacity profile on atmospheric properties, we developed a TES limb-scan observation-based three-dimensional and time-evolving dust climatology for use in forcing general circulation models (GCMs). We use this to force the MarsWRF GCM and compare with simulations that use a well-mixed (Conrath-) vertical dust profile and Mars Climate Database version 4 (MCD) horizontal distribution dust opacity forcing function. We find that simulated temperatures using the TES-derived forcing yield a 1.18 standard deviation closer match to TES temperature retrievals than a MarsWRF simulation using MCD forcing. The climatological forcing yields significant changes to many large-scale features of the simulated atmosphere. Notably the high-latitude westerly jet speeds are 10-20m/s higher, polar warming collar temperatures are 20-30K warmer near northern winter solstice and tilted more strongly poleward, the middle and lower atmospheric meridional circulations are partially decoupled, the migrating diurnal tide exhibits destructive interference and is weakened by 50% outside of equinox, and the southern hemisphere wave number 1 stationary wave is strengthened by up to 4K (45%). We find the vertical dust distribution is an important factor for Martian lower and middle atmospheric thermal structure and circulation that cannot be neglected in analysis and simulation of the Martian atmosphere. C1 [Guzewich, Scott D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Toigo, Anthony D.; Talaat, Elsayed R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Richardson, Mark I.; Newman, Claire E.] Ashima Res, Pasadena, CA USA. [Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [McConnochie, Timothy H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Guzewich, SD (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Bldg 34, Greenbelt, MD 20771 USA. EM scott.d.guzewich@nasa.gov RI Waugh, Darryn/K-3688-2016; OI Waugh, Darryn/0000-0001-7692-2798; Guzewich, Scott/0000-0003-1149-7385 FU Johns Hopkins University Applied Physics Laboratory graduate student fellowship FX This work was funded by a Johns Hopkins University Applied Physics Laboratory graduate student fellowship. We thank R. John Wilson and Jean-Baptiste Madeleine for helpful reviews which have improved and clarified this work. NR 76 TC 11 Z9 11 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY PY 2013 VL 118 IS 5 BP 980 EP 993 DI 10.1002/jgre.20084 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400009 ER PT J AU Parsons, RA Moore, JM Howard, AD AF Parsons, R. A. Moore, J. M. Howard, A. D. TI Evidence for a short period of hydrologic activity in Newton crater, Mars, near the Hesperian-Amazonian transition SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; water; alluvial fan; climate; sediment; channel ID LARGE ALLUVIAL FANS; AQUEOUS SEDIMENTATION; VALLES MARINERIS; SUMMIT SNOWPACK; DELTA FORMATION; WATER; TRANSPORT; CHANNELS; ORIGIN; FLOW AB Hesperian/Amazonian-aged valleys and alluvial fans distributed in regional clusters throughout the southern middle- to low-latitudes were formed during a period of fluvial runoff and erosion which acted over a smaller spatial and temporal scale than the older, classical Martian valley networks dated to the Noachian-Hesperian boundary. In order to explore the potential sources of water which formed these younger valleys, we calculated the expected sediment transport and water discharge rates for a valley and alluvial fan located in Newton crater (40 degrees S, -159 degrees E) over a wide range of water-filled channel depths and sediment grain sizes in order to constrain the formation timescale and required water volume. Depending on the depth of the water-filled channel within the valley, the alluvial fan was likely emplaced over approximate to 0.1 to approximate to 10years of fluvial activity involving between 1.8 and 5.7km (3) of water. These results imply water runoff rates of between 1 and 10cm/d over a typical 300km(2) drainage area. Possible processes for delivering water to these drainages include high obliquity snowpack melting via volcanism or impacts resulting in either scattered, local to regional melting events or a brief global warming event. An extended, perhaps episodic, period of fluvial activity lasting hundreds of years driven by insolation-induced melting of high obliquity snowpacks is another possibility. C1 [Parsons, R. A.; Moore, J. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Howard, A. D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. RP Parsons, RA (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM reid.a.parsons@nasa.gov OI Howard, Alan/0000-0002-5423-1600 FU NASA Postdoctoral Program at the Ames Research Center; NASA's Mars Data Analysis Program; NASA FX This research was supported by an appointment of the first author to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. J. M. Moore and A. D. Howard were supported by a grant from NASA's Mars Data Analysis Program. The authors would like to thank Francis Nimmo for his support of the initial work for this project, Ross Beyer for providing technical assistance with ISIS, and Brian Hynek for sharing his valley network data. This manuscript benefited from constructive reviews from Cathy Quantin and an anonymous reviewer. NR 61 TC 4 Z9 4 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY PY 2013 VL 118 IS 5 BP 1082 EP 1093 DI 10.1002/jgre.20088 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400015 ER PT J AU Farrell, WM Poppe, AR Zimmerman, MI Halekas, JS Delory, GT Killen, RM AF Farrell, W. M. Poppe, A. R. Zimmerman, M. I. Halekas, J. S. Delory, G. T. Killen, R. M. TI The lunar photoelectron sheath: A change in trapping efficiency during a solar storm SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Moon; photoelectrons; sheath; coronal mass ejection ID MAGNETIC-FIELDS; SPACE; DUST AB On the lunar dayside, photoelectrons are quasi-constantly emitted from the Moon's surface and this electron flux acts to typically charge the dayside lunar surface a few volts positive. In arriving at an equilibrium surface potential, the surface will charge to balance the two primary currents: the outgoing photoelectron flux, J(p), against the incoming solar wind electron thermal flux, J(e). In nominal solar wind conditions, J(p)>J(e) and the surface charges positive, trapping most of the photoelectrons. However, during the passage of a coronal mass ejection (CME), the incoming electron thermal flux, J(e), will quickly change from being less than J(p) to being greater than J(p) on time scales of similar to 1-2% of a lunation. Using a set of independently developed particle-in-cell plasma codes, we find at times when J(p)/J(e) < 1, there is substantially less near-surface electrostatic trapping of the photoelectrons due to the reduction of the restraining surface potential. The photoelectron population then has almost direct access to upstream regions. We find that the morphology of the sheath is very different in the CME's dense cool plasma than in the nominal solar wind, with a larger relative portion of the photoelectrons now liberated to propagate upstream into plasma regions ahead of the Moon. C1 [Farrell, W. M.; Zimmerman, M. I.; Killen, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Poppe, A. R.; Halekas, J. S.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Zimmerman, M. I.] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Farrell, W. M.; Poppe, A. R.; Zimmerman, M. I.; Halekas, J. S.; Delory, G. T.; Killen, R. M.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM William.M.Farrell@nasa.gov RI Farrell, William/I-4865-2013; OI Halekas, Jasper/0000-0001-5258-6128 NR 21 TC 6 Z9 6 U1 0 U2 7 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 MAY PY 2013 VL 118 IS 5 BP 1114 EP 1122 DI 10.1002/jgre.20086 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400017 ER PT J AU Poppe, AR Halekas, JS Samad, R Sarantos, M Delory, GT AF Poppe, A. R. Halekas, J. S. Samad, R. Sarantos, M. Delory, G. T. TI Model-based constraints on the lunar exosphere derived from ARTEMIS pickup ion observations in the terrestrial magnetotail SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE lunar exosphere; pick-up ions; terrestrial magnetotail; micrometeoroid bombardment; surface charging ID ATMOSPHERE; MOON; SURFACE; SODIUM; INSTRUMENT AB We use Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) measurements of lunar exospheric pickup ions in the terrestrial magnetotail lobes combined with a particle-tracing model to constrain the source species and distributions of the lunar neutral exosphere. These pickup ions, generated by photoionization of neutral species while the Moon is in the magnetotail lobes, undergo acceleration from both the magnetotail convection electric field and the lunar surface photoelectric field, giving rise to distinct pickup ion flux, pitch angle, and energy distributions. By simulating the behavior of lunar pickup ions in the magnetotail lobes and the response of the twin ARTEMIS probes under various ambient conditions, we can constrain several physical quantities associated with these observations, including the source ion production rate and the magnetotail convection velocity (and hence, electric field). Using the model-derived source ion production rate and established photoionization rates, we present upper limits on the density of several species potentially in the lunar exosphere. In certain cases, these limits are lower than those previously reported. We also present evidence that the lunar exosphere is displaced toward the lunar dawnside while in the terrestrial magnetotail based on fits to the observed pickup ion distributions. C1 [Poppe, A. R.; Halekas, J. S.; Samad, R.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Poppe, A. R.; Halekas, J. S.; Sarantos, M.; Delory, G. T.] NASA, Lunar Sci Inst, Ames Res Ctr, Mountain View, CA USA. [Sarantos, M.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, CA USA. [Sarantos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM poppe@ssl.berkeley.edu OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128 FU NASA's Lunar Science Institute; NASA [NAS5-02099]; NASA's LASER program [NNX13AJ97G] FX The authors gratefully acknowledge support from NASA's Lunar Science Institute and acknowledge NASA contract NAS5-02099 for THEMIS/ARTEMIS support. A. R. P and J. S. H. also acknowledge support from NASA's LASER program, grant #NNX13AJ97G. We thank J.P. McFadden for the use of THEMIS ESA data in support of this research. We thank the Photo-Rate Data Coefficient Data Base [http://phidrates.space.swri.edu] and the LASP LISIRD site [http://lasp.colorado.edu/lisird/missiondatafiles.html] for access to cross sections and solar spectra used to calculate photoionizations rates. NR 46 TC 6 Z9 6 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY PY 2013 VL 118 IS 5 BP 1135 EP 1147 DI 10.1002/jgre.20090 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400019 ER PT J AU Clancy, RT Sandor, BJ Wolff, MJ Smith, MD Lefevre, F Madeleine, JB Forget, F Murchie, SL Seelos, FP Seelos, KD Nair, H Toigo, AD Humm, D Kass, DM Kleinbohl, A Heavens, N AF Clancy, R. Todd Sandor, Brad J. Wolff, Michael J. Smith, Michael D. Lefevre, Franck Madeleine, Jean-Baptiste Forget, Francois Murchie, Scott L. Seelos, Frank P. Seelos, Kim D. Nair, Hari Toigo, Anthony D. Humm, David Kass, David M. Kleinboehl, Armin Heavens, Nicholas TI Extensive MRO CRISM observations of 1.27 mu m O-2 airglow in Mars polar night and their comparison to MRO MCS temperature profiles and LMD GCM simulations (vol 117, E00J10, 2012) SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Correction DE Correction; Mars; Nightglow; O2; Atmosphere; Photochemistry C1 [Clancy, R. Todd; Sandor, Brad J.; Wolff, Michael J.] Space Sci Inst, Boulder, CO USA. [Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lefevre, Franck] Lab Atmospheres Milieux Observat Spatiales, Paris, France. [Madeleine, Jean-Baptiste; Forget, Francois] Meteorol Dynam Lab, Paris, France. [Murchie, Scott L.; Seelos, Frank P.; Seelos, Kim D.; Nair, Hari; Toigo, Anthony D.; Humm, David] Johns Hopkins Univ, Appl Phys Lab, Columbia, MD USA. [Kleinboehl, Armin] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Heavens, Nicholas] Hampton Univ, Hampton, VA 23668 USA. RP Clancy, RT (reprint author), Space Sci Inst, Boulder, CO USA. EM clancy@spacescience.org RI Murchie, Scott/E-8030-2015; Seelos, Kimberly/F-4647-2015; Humm, David/B-8825-2016; Seelos, Frank/C-7875-2016 OI Murchie, Scott/0000-0002-1616-8751; Seelos, Kimberly/0000-0001-7236-0580; Humm, David/0000-0003-1520-261X; Seelos, Frank/0000-0001-9721-941X NR 3 TC 3 Z9 3 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY PY 2013 VL 118 IS 5 BP 1148 EP 1154 DI 10.1002/jgre.20073 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400020 ER PT J AU Smith, MWE Fox, DB Cowen, DF Meszaros, P Tesic, G Fixelle, J Bartos, I Sommers, P Ashtekar, A Babu, GJ Barthelmy, SD Coutu, S DeYoung, T Falcone, AD Gao, S Hashemi, B Homeier, A Marka, S Owen, BJ Taboada, I AF Smith, M. W. E. Fox, D. B. Cowen, D. F. Meszaros, P. Tesic, G. Fixelle, J. Bartos, I. Sommers, P. Ashtekar, Abhay Babu, G. Jogesh Barthelmy, S. D. Coutu, S. DeYoung, T. Falcone, A. D. Gao, Shan Hashemi, B. Homeier, A. Marka, S. Owen, B. J. Taboada, I. TI The Astrophysical Multimessenger Observatory Network (AMON) SO ASTROPARTICLE PHYSICS LA English DT Article DE High-energy astrophysics; Gravitational radiation; Neutrinos; Cosmic rays; Gamma-ray bursts; Supernovae ID GAMMA-RAY BURSTS; PRIMORDIAL BLACK-HOLES; HIGH-ENERGY NEUTRINOS; LARGE-AREA TELESCOPE; SUPERSYMMETRIC DARK-MATTER; GRAVITATIONAL-WAVE BURSTS; TEV BLAZAR 1ES-1959+650; GLUON-JET EMISSION; COSMIC-RAYS; RELATIVISTIC JETS AB We summarize the science opportunity, design elements, current and projected partner observatories, and anticipated science returns of the Astrophysical Multimessenger Observatory Network (AMON). AMON will link multiple current and future high-energy, multimessenger, and follow-up observatories together into a single network, enabling near real-time coincidence searches for multimessenger astrophysical transients and their electromagnetic counterparts. Candidate and high-confidence multimessenger transient events will be identified, characterized, and distributed as AMON alerts within the network and to interested external observers, leading to follow-up observations across the electromagnetic spectrum. In this way, AMON aims to evoke the discovery of multimessenger transients from within observatory subthreshold data streams and facilitate the exploitation of these transients for purposes of astronomy and fundamental physics. As a central hub of global multimessenger science, AMON will also enable cross-collaboration analyses of archival datasets in search of rare or exotic astrophysical phenomena. (C) 2013 Elsevier B.V. All rights reserved. C1 [Smith, M. W. E.; Cowen, D. F.; Meszaros, P.; Tesic, G.; Sommers, P.; Ashtekar, Abhay; Coutu, S.; DeYoung, T.; Gao, Shan; Hashemi, B.; Owen, B. J.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Smith, M. W. E.; Fox, D. B.; Cowen, D. F.; Meszaros, P.; Tesic, G.; Sommers, P.; Ashtekar, Abhay; Coutu, S.; DeYoung, T.; Falcone, A. D.; Gao, Shan; Owen, B. J.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Fox, D. B.; Cowen, D. F.; Meszaros, P.; Fixelle, J.; Sommers, P.; Babu, G. Jogesh; Falcone, A. D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bartos, I.; Marka, S.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Bartos, I.; Marka, S.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Babu, G. Jogesh] Penn State Univ, Dept Stat, University Pk, PA 16802 USA. [Barthelmy, S. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Homeier, A.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Taboada, I.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. RP Smith, MWE (reprint author), Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA. EM msmith@gravity.psu.edu; dfox@astro.psu.edu; cowen@phys.psu.edu; nnp@astro.psu.edu; gut10@psu.edu; jxf5078@psu.edu; ibartos@phys.columbia.edu; sommers@phys.psu.edu; ashtekar@gravity.psu.edu; babu@psu.edu; scott.d.barthelmy@nasa.gov; coutu@phys.psu.edu; deyoung@phys.psu.edu; afalcone@astro.psu.edu; sxg324@psu.edu; bth5032@psu.edu; homeier@physik.uni-bonn.de; sm2375@columbia.edu; owen@gravity.psu.edu; itaboada@gatech.edu RI Bartos, Imre/A-2592-2017 FU Penn State's Office of the Senior Vice President for Research; Eberly College of Science; Penn State Institute for Gravitation; Cosmos; Penn State Institute for CyberScience Faculty Fellows Program; Columbia University; National Science Foundation [PHY-0847182] FX Initial development of AMON has been funded by Penn State's Office of the Senior Vice President for Research, the Eberly College of Science, and the Penn State Institute for Gravitation and the Cosmos. D. F. Cowen acknowledges the support of the Penn State Institute for CyberScience Faculty Fellows Program; I. Bartos and S. Marka acknowledge support from Columbia University and the National Science Foundation under cooperative agreement PHY-0847182. NR 115 TC 12 Z9 13 U1 1 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD MAY PY 2013 VL 45 BP 56 EP 70 DI 10.1016/j.astropartphys.2013.03.003 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 212VJ UT WOS:000324010600007 ER PT J AU Daigle, MJ Goebel, K AF Daigle, Matthew J. Goebel, Kai TI Model-Based Prognostics With Concurrent Damage Progression Processes SO IEEE TRANSACTIONS ON SYSTEMS MAN CYBERNETICS-SYSTEMS LA English DT Article DE Centrifugal pumps; model-based prognostics; particle filters; variance control ID FAILURE PROGNOSIS; DIAGNOSIS; TRACKING; SYSTEM AB Model-based prognostics approaches rely on physics-based models that describe the behavior of systems and their components. These models must account for the several different damage processes occurring simultaneously within a component. Each of these damage and wear processes contributes to the overall component degradation. We develop a model-based prognostics methodology that consists of a joint state-parameter estimation problem, in which the state of a system along with parameters describing the damage progression are estimated, followed by a prediction problem, in which the joint state-parameter estimate is propagated forward in time to predict end of life and remaining useful life. The state-parameter estimate is computed using a particle filter and is represented as a probability distribution, allowing the prediction of end of life and remaining useful life within a probabilistic framework that supports uncertainty management. We also develop a novel variance control algorithm that maintains an uncertainty bound around the unknown parameters to limit the amount of estimation uncertainty and, consequently, reduce prediction uncertainty. We construct a detailed physics-based model of a centrifugal pump that includes damage progression models, to which we apply our model-based prognostics algorithm. We illustrate the operation of the prognostic solution with a number of simulation-based experiments and demonstrate the performance of the approach when multiple damage mechanisms are active. C1 [Daigle, Matthew J.; Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Daigle, MJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM matthew.j.daigle@nasa.gov; kai.goebel@nasa.gov OI Daigle, Matthew/0000-0002-4616-3302 FU NASA Fault Detection, Isolation, and Recovery (FDIR) project; NASA System-wide Safety and Assurance Technologies (SSAT) project FX Manuscript received September 6, 2011; revised March 28, 2012; accepted June 5, 2012. Date of publication September 12, 2012; date of current version April 12, 2013. This work was supported by the NASA Fault Detection, Isolation, and Recovery (FDIR) and System-wide Safety and Assurance Technologies (SSAT) projects. This paper was recommended by Associate Editor G. Biswas. NR 31 TC 28 Z9 28 U1 0 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2168-2216 J9 IEEE T SYST MAN CY-S JI IEEE Trans. Syst. Man Cybern. -Syst. PD MAY PY 2013 VL 43 IS 3 BP 535 EP 546 DI 10.1109/TSMCA.2012.2207109 PG 12 WC Automation & Control Systems; Computer Science, Cybernetics SC Automation & Control Systems; Computer Science GA 206CZ UT WOS:000323495900005 ER PT J AU Sharp, ZD Draper, DS AF Sharp, Z. D. Draper, D. S. TI The chlorine abundance of Earth: Implications for a habitable planet SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Cl; chlorine; Earth composition; meteorite; planetary formation; core composition ID EARLY CHEMICAL HISTORY; SOLAR NEBULA; ISOTOPE COMPOSITION; ELEMENT CHEMISTRY; ALLENDE METEORITE; VOLATILE CONTENT; EARLY EVOLUTION; GIANT IMPACT; MANTLE; SYSTEM AB The Cl, Br and I contents of Earth are depleted by a factor of 10 relative to predicted values from chondritic and solar abundances. Possible explanations for the apparent discrepancy include (1) unrecognized sequestration of Cl in the core, (2) a much higher nebular volatility than normally presumed or (3) a preferential loss of the heavy halogens during planetary accretion. We tested the first assumption by conducting high pressure-temperature equilibration experiments between silicate and metal. At 15 GPa and 1900 degrees C, the DCl(metal-silicate) value for Cl is less than 0.007, indicating that the core is not a significant reservoir for Cl. The concentration of Cl in all chondritic classes follows a depletion trend very similar to that of Na and Mn, arguing against a low condensation temperature for Cl. Instead, we propose that the depletion of the heavy halogens is due to their unique hydrophilic behavior. Almost half of Earth's Cl and Br inventory resides in the ocean and evaporites, demonstrating the unique affinity for aqueous solutions for these elements. During planetary accretion, there would have been a strong sequestration of halogens into the crustal reservoir. 'Collisional erosion' during planetary accretion provides a mechanism that would uniquely strip the heavy halogens out of an accreting Earth. Had such loss not occurred, the salinity of the oceans would be 10 x the present value, and complex life would probably never have evolved. (C) 2013 Elsevier B.V. All rights reserved. C1 [Sharp, Z. D.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Draper, D. S.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. RP Sharp, ZD (reprint author), Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. EM zsharp@unm.edu FU NASA; Alexander von Humboldt fellowship FX We would like to thank Carl Agee for access to the UNM High Pressure laboratory and Hugh O'Neill for his helpful insights. James Brenan and Ray Burgess provided very helpful reviews of the manuscript. Funding was provided by NASA grant and an Alexander von Humboldt fellowship to Sharp. NR 65 TC 17 Z9 17 U1 7 U2 50 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 MAY PY 2013 VL 369 BP 71 EP 77 DI 10.1016/j.epsl.2013.03.005 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 168CY UT WOS:000320684500007 ER PT J AU Nguyen, TV Nosratinia, A Divsalar, D AF Thuy Van Nguyen Nosratinia, Aria Divsalar, Dariush TI Bilayer Protograph Codes for Half-Duplex Relay Channels SO IEEE TRANSACTIONS ON WIRELESS COMMUNICATIONS LA English DT Article DE Relay channel; LDPC codes; protograph codes; multiple-relay channel ID PARITY-CHECK CODES; LDPC CODES; CAPACITY THEOREMS; DESIGN AB Despite encouraging advances in the design of relay codes, several important challenges remain. Many of the existing LDPC relay codes are tightly optimized for fixed channel conditions and not easily adapted without extensive re-optimization of the code. Some have high encoding complexity and some need long block lengths to approach capacity. This paper presents a high-performance protograph-based LDPC coding scheme for the half-duplex relay channel that addresses simultaneously several important issues: structured coding that permits easy design, low encoding complexity, embedded structure for convenient adaptation to various channel conditions, and performance close to capacity with a reasonable block length. The application of the coding structure to multi-relay networks is demonstrated. Finally, a simple new methodology for evaluating the end-to-end error performance of relay coding systems is developed and used to highlight the performance of the proposed codes. C1 [Thuy Van Nguyen; Nosratinia, Aria] Univ Texas Dallas, Dept Elect Engn, Richardson, TX 75083 USA. [Divsalar, Dariush] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nguyen, TV (reprint author), Univ Texas Dallas, Dept Elect Engn, Richardson, TX 75083 USA. EM nvanthuy@utdallas.edu; aria@utdallas.edu; Dar-iush.Divsalar@jpl.nasa.gov OI Nosratinia, Aria/0000-0002-3751-0165 FU VOSP program from the Ministry of Education and Training, Vietnam; THECB [009741-0084-2007]; NASA FX This research was supported in part by the VOSP program from the Ministry of Education and Training, Vietnam, and in part by the grant 009741-0084-2007 from THECB. This research was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 27 TC 4 Z9 4 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1536-1276 EI 1558-2248 J9 IEEE T WIREL COMMUN JI IEEE Trans. Wirel. Commun. PD MAY PY 2013 VL 12 IS 5 BP 1969 EP 1977 DI 10.1109/TWC.2013.040413.111745 PG 9 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 175AA UT WOS:000321199800001 ER PT J AU Langmore, I Davis, AB Bal, G AF Langmore, Ian Davis, Anthony B. Bal, Guillaume TI Multipixel Retrieval of Structural and Optical Parameters in a 2-D Scene With a Path-Recycling Monte Carlo Forward Model and a New Bayesian Inference Engine SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Algorithm design and analysis; Bayesian methods; computational efficiency; computational geometry; hyperspectral imaging; Markov processes; maximum a posteriori estimation; radiometry; remote monitoring; signal processing algorithms; surface topography ID POINT-SPREAD FUNCTION; RADIATIVE-TRANSFER; ATMOSPHERIC TRANSFER; SURFACE ALBEDO; REFLECTION; OBJECTIVES; SIMULATION; SCATTERING; SCIENCE; MISSION AB Physics-based retrievals of atmosphere and/or surface properties are generally multi- or hyperspectral in nature; some use multi-angle information as well. Recently, polarization has been added to the available input from sensors and accordingly modeled with vector radiative transfer (RT). At any rate, a single pixel is processed at a time using a forward RT model predicated on 1-D transport theory. Neighboring pixels are sometimes considered but, generally, just to formulate statistical constraints on the inversion based on spatial context. Herein, we demonstrate the power to be harnessed by adding bona fide multipixel techniques to the mix. We use a forward RT model in 2-D, sufficient for this demonstration and easily extended to 3-D, for the response of a single-wavelength imaging sensor. The data, an image, is used to infer position, size, and opacity of an absorbing atmospheric plume somewhere in a deep valley in the presence of partially known/partially unknown aerosol. We first describe the necessary innovation to speed-up forward multidimensional RT. In spite of its reputation for inefficiency, we use a Monte Carlo (MC) technique. However, the adopted scheme is highly accelerated without loss of accuracy by using "recycled" MC paths. This forward model is then put to work in a novel Bayesian inversion adapted to this kind of RT model where it is straightforward to trade precision and efficiency. Retrievals target the plume properties and the specific amount of aerosol. In spite of the limited number of pixels and low signal-to-noise ratio, there is added value for certain nuclear treaty verification applications. C1 [Langmore, Ian; Bal, Guillaume] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. [Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Langmore, I (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. EM ianlangmore@gmail.com; Anthony.B.Davis@jpl.nasa.gov; gb2030@columbia.edu FU Department of Energy [DE-FG52-08NA28779]; National Science Foundation [DMS-0804696] FX Manuscript received November 22, 2011; revised July 9, 2012; accepted August 19, 2012. Date of publication November 20, 2012; date of current version April 18, 2013. This research was supported by the Department of Energy under Grant DE-FG52-08NA28779 (to Columbia and the Jet Propulsion Laboratory) and the National Science Foundation under Grant DMS-0804696 (to Columbia University). NR 51 TC 3 Z9 3 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAY PY 2013 VL 51 IS 5 BP 2903 EP 2919 DI 10.1109/TGRS.2012.2217380 PN 2 PG 17 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 171OY UT WOS:000320940000001 ER PT J AU Mazaheri, A Johnston, CO Sefidbakht, S AF Mazaheri, Alireza Johnston, Christopher O. Sefidbakht, Siavash TI Three-Dimensional Radiation Ray-Tracing for Shock-Layer Radiative Heating Simulations SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID TRANSPORT; APPROXIMATION AB A three-dimensional ray-tracing algorithm is developed for shock-layer radiative heating predictions. When coupled with a tangent slab approximate code, such as the HARA radiation code, this algorithm provides an efficient approach for computing the radiative heating and allows the commonly applied tangent slab approximation to be removed. Application to several Earth- and Mars-entry conditions show that the ray-tracing approach predicts up to 15% lower radiative heating values than the tangent slab approximation at the stagnation point, which is consistent with the results of previous studies. In the afterbody region of Mars entry vehicles, where radiative heating from the CO2 molecule may be larger than convective heating, a 70% reduction from the tangent-slab result is seen, indicating the inadequacy of the tangent slab approximation in such regions. C1 [Mazaheri, Alireza; Johnston, Christopher O.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Sefidbakht, Siavash] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Mazaheri, A (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, M-S 408A, Hampton, VA 23681 USA. EM Ali.R.Mazaheri@nasa.gov FU Hypersonic Inflatable Aerodynamic Decelerators program; NASA fundamental aeronautics program; NASA Langley Aerothermodynamics Branch through the NASA Langley Research Summer Student program FX The authors would like to thank Lin Hartung for her help during the algorithm development. The thanks should also go to the Hypersonic Inflatable Aerodynamic Decelerators program for partial support of the first author. The NASA fundamental aeronautics program funded the second's author work. The NASA Langley Aerothermodynamics Branch funded the third author's work through the NASA Langley Research Summer Student program. NR 26 TC 3 Z9 3 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS 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 MAY-JUN PY 2013 VL 50 IS 3 BP 485 EP 493 DI 10.2514/1.A32448 PG 9 WC Engineering, Aerospace SC Engineering GA 160BM UT WOS:000320091200001 ER PT J AU Reda, DC Wilder, MC Prabhu, DK AF Reda, Daniel C. Wilder, Michael C. Prabhu, Dinesh K. TI Transition Experiments on Blunt Cones with Distributed Roughness in Hypersonic Flight SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 50th AIAA Aerospace Sciences Meeting and Exhibit including the New Horizons Forum and Aerospace Exposition CY JAN 06-13, 2012 CL Nashville, TN SP AIAA, US AF Off Sci Res ID BOUNDARY-LAYER-TRANSITION AB Blunt cones with smooth nosetips and roughened frusta were flown in the NASA Ames Research Center hypersonic ballistic range at a Mach number of 10 through quiescent air environments. Global surface temperature distributions were optically measured and analyzed to determine transition onset and progression over the roughened frusta. Real-gas Navier-Stokes calculations of model flowfields, including laminar boundary-layer development in these flowfields, were conducted to predict values of key dimensionless parameters used to correlate transition on such configurations in hypersonic flow. It was found that nose bluntness has a major influence on roughness-induced transition onset and progression. For small-bluntness cones, pretest computations showed that values of the roughness Reynolds number increased with increasing distance from the beginning of the roughness elements. Transition onset was first observed on the roughened frusta near the cone base, and the transition front progressed forward with increasing freestream pressure at a constant value of the critical roughness Reynolds number. Conversely, for large-bluntness cones, pretest computations showed that values of the roughness Reynolds number decreased with increasing distance from the beginning of the roughness. Transition onset was again observed near the cone base, but forward progression of the transition front with increasing freestream pressure occurred at ever-increasing values of the roughness Reynolds number, a response characteristic of breakdown to turbulence downstream of a "trip ring" or "trip array." C1 [Reda, Daniel C.; Wilder, Michael C.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA. [Prabhu, Dinesh K.] ERC Inc, Moffett Field, CA 94035 USA. RP Reda, DC (reprint author), NASA, Ames Res Ctr, Aerothermodynam Branch, MS 230-2, Moffett Field, CA 94035 USA. NR 8 TC 1 Z9 1 U1 1 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS 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 MAY-JUN PY 2013 VL 50 IS 3 BP 504 EP 508 DI 10.2514/1.A32426 PG 5 WC Engineering, Aerospace SC Engineering GA 160BM UT WOS:000320091200003 ER PT J AU Mehta, M Canabal, F Tashakkor, SB Smith, SD AF Mehta, Manish Canabal, Francisco Tashakkor, Scott B. Smith, Sheldon D. TI Numerical Base Heating Sensitivity Study for a Four-Rocket Engine Core Configuration SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB In support of launch vehicle plume-induced base heating and pressure prediction efforts using the Loci-CHEM Navier-Stokes computational fluid dynamics solver, numerical simulations of a wind-tunnel test have been modeled and analyzed. This missile forebody test article is composed of four JP-4/LOX 500 lbf water-cooled rocket engines exhausting into a Mach 2-3.5 wind tunnel at various freestream pressure conditions. This study explores the base heating sensitivity for varying boundary conditions and various chemistry, turbulence, and thermodynamic models. The numerical solutions have been investigated at two freestream pressure conditions: 255 lb/ft(2) (simulated low altitude) and 35 lb/ft(2) (simulated high altitude). It is observed that the convective base heat flux and base temperature are most sensitive to the nozzle inner wall thermal boundary-layer profile, which is dependent on the wall temperature, boundary layer's specific energy, jet expansion ratio, and chemical reactions. Recovery shock and wall jet dynamics and afterburning within the updraft plume also significantly influence convective base heating. Turbulence modeling shows less sensitivity to base heating characteristics. Base heating rates are validated for the highest-fidelity predictions, which show an agreement within 10% with respect to test data. C1 [Mehta, Manish; Canabal, Francisco] NASA, Marshall Space Flight Ctr, Aerosci Branch, Huntsville, AL 35812 USA. [Tashakkor, Scott B.] Jacobs Engn Sci & Tech Serv Grp, Aerosci Branch, Huntsville, AL 35812 USA. [Smith, Sheldon D.] Jacobs Engn Sci & Tech Serv Grp Plumetech, Aerosci Branch, Huntsville, AL 35812 USA. RP Mehta, M (reprint author), NASA, Marshall Space Flight Ctr, Aerosci Branch, MS 3418-EV33, Huntsville, AL 35812 USA. EM manish.mehta@nasa.gov NR 30 TC 0 Z9 0 U1 1 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2013 VL 50 IS 3 BP 509 EP 526 DI 10.2514/1.A32287 PG 18 WC Engineering, Aerospace SC Engineering GA 160BM UT WOS:000320091200004 ER PT J AU Oh, DY Landau, D AF Oh, David Y. Landau, Damon TI Simple Semi-Analytic Model for Optimized Interplanetary Low-Thrust Trajectories Using Solar Electric Propulsion SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 46th AIAA/ASME/SAE/ASEE Joint Propulsion Conference and Exhibit CY JUL 25-29, 2010 CL Nashville, TN SP AIAA, ASME, SAE, ASEE, Israel Minist Sci, Culture & Sport AB This paper describes a simple semi-analytic model for mass-optimized interplanetary solar electric low-thrust trajectories. A description is given of a model that accurately and quickly determines the performance of circular-coplanar low-thrust transfers with a series of simple empirical and physics-based relationships that can be implemented easily in a spreadsheet. The model takes flight time, departure and arrival velocity, initial power, initial mass, and propulsion-system efficiency as inputs and produces the optimum specific impulse, A v, final mass, and burn time that correspond to the mass-optimum trajectory as outputs. The development methodology is described, governing variables and fundamental relationships are identified, and a model is presented that efficiently calculates these parameters for a wide range of low-thrust trajectories. Models are presented for Earth-Jupiter/Trojan asteroid, Earth-Mars, Mars-Earth, Earth-Venus, and Earth-Main-Belt asteroid transfers using solar electric propulsion. The results show good agreement for estimates of both delivered mass (+8/-15%) and optimum specific impulse (+20/-20%). This model is well suited to classroom instruction, concurrent engineering, and the initial development of new mission concepts. C1 [Oh, David Y.] CALTECH, Jet Prop Lab, Mars Sci Lab, Project Syst Engn, Pasadena, CA 91109 USA. [Landau, Damon] CALTECH, Jet Prop Lab, Outer Planet Mission Anal Grp, Pasadena, CA 91109 USA. RP Oh, DY (reprint author), CALTECH, Jet Prop Lab, Mars Sci Lab, Project Syst Engn, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM david.y.oh@jpl.nasa.gov; Damon.Landau@jpl.nasa.gov NR 14 TC 2 Z9 2 U1 1 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS 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 MAY-JUN PY 2013 VL 50 IS 3 BP 609 EP 619 DI 10.2514/1.A32326 PG 11 WC Engineering, Aerospace SC Engineering GA 160BM UT WOS:000320091200012 ER PT J AU Karlgaard, CD Beck, RE Derry, SD Brandon, JM Starr, BR Tartabini, PV Olds, AD AF Karlgaard, Christopher D. Beck, Roger E. Derry, Stephen D. Brandon, Jay M. starr, Brett R. Tartabini, Paul V. Olds, Aaron D. TI Ares I-X Trajectory Reconstruction: Methodology and Results SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA Atmospheric Flight Mechanics Conference / AIAA Modeling and Simulation Technologies Conference / AIAA Guidance Navigation and Control Conference CY AUG 08-11, 2011 CL Portland, OR SP AIAA AB The Ares I-X trajectory reconstruction produced best-estimated trajectories of the flight-test vehicle ascent through stage separation and of the first- and upper-stage entries after separation. The trajectory-reconstruction process combines onboard, ground-based, and atmospheric measurements to produce the trajectory estimates, using an iterated extended Kalman filter algorithm. The Ares I-X vehicle had a number of onboard and ground-based sensors that were available, including inertial measurement units, radar, air data, and weather balloons. However, due to problems with calibrations and/or data, not all of the sensor data were used. This paper describes the methodology and results of the trajectory-reconstruction process, including flight-data preprocessing and input uncertainties, trajectory-estimation algorithms and dynamic models, output transformations, and comparisons with preflight predictions. The results of the reconstruction indicate nominal vehicle performance that is well within the range of expected dispersions based on preflight Monte Carlo analysis. C1 [Karlgaard, Christopher D.; Olds, Aaron D.] Analyt Mech Associates Inc, Hampton, VA 23666 USA. [Beck, Roger E.] Analyt Mech Associates Inc, Huntsville, AL 35806 USA. [Derry, Stephen D.] NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA. [Brandon, Jay M.] NASA, Langley Res Ctr, Flight Dynam Branch, Hampton, VA 23681 USA. [starr, Brett R.; Tartabini, Paul V.] NASA, Langley Res Ctr, Vehicle Anal Branch, Hampton, VA 23681 USA. RP Karlgaard, CD (reprint author), Analyt Mech Associates Inc, Hampton, VA 23666 USA. NR 32 TC 7 Z9 7 U1 0 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS 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 MAY-JUN PY 2013 VL 50 IS 3 BP 641 EP 661 DI 10.2514/1.A32345 PG 21 WC Engineering, Aerospace SC Engineering GA 160BM UT WOS:000320091200015 ER PT J AU Crespo, LG Kenny, SP Giesy, DP AF Crespo, Luis G. Kenny, Sean P. Giesy, Daniel P. TI Reliability analysis of polynomial systems subject to p-box uncertainties SO MECHANICAL SYSTEMS AND SIGNAL PROCESSING LA English DT Article DE Imprecise probabilities; Reliability analysis; Bernstein polynomials; Extreme-case distributions; p-Boxes ID EPISTEMIC UNCERTAINTY; GLOBAL OPTIMIZATION; PROGRAMS; BOUNDS AB This paper proposes a reliability analysis framework for systems subject to multiple design requirements that depend polynomially on uncertain parameters. The values these polynomials take at a given realization of the uncertain parameters dictate whether that realization is a failure or a success point. In this paper, reliability analysis refers to the estimation or bounding of the probability of failure for a given model of the uncertainty. The probability distributions of the uncertain parameters are presumed to belong to a given probability box (also known as a p-box). This does not give sufficient information to determine the failure probability of such a system exactly, but does limit the range of values it might take. Two techniques for bounding this range are proposed herein. In the first approach, we calculate the p-box of the requirements functions by propagating all the hyper-rectangles defined by the p-box of the uncertain parameters. In the second approach, we find inner bounding sets of the safe and failure domains and search for the elements of the p-box that minimize and maximize the probability of such sets. Iterative refinement of the bounding sets allows tightening arbitrarily closely the offset between the actual failure probability range and the calculated outer bound. In both techniques, bounds of the functions describing the design requirements over hyper-rectangular sets are calculated and iteratively refined by expanding them using Bernstein bases. Published by Elsevier Ltd. C1 [Crespo, Luis G.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Kenny, Sean P.; Giesy, Daniel P.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Crespo, LG (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM Luis.G.Crespo@nasa.gov NR 20 TC 8 Z9 8 U1 0 U2 6 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0888-3270 J9 MECH SYST SIGNAL PR JI Mech. Syst. Signal Proc. PD MAY-JUN PY 2013 VL 37 IS 1-2 SI SI BP 121 EP 136 DI 10.1016/j.ymssp.2012.08.012 PG 16 WC Engineering, Mechanical SC Engineering GA 148GJ UT WOS:000319232200010 ER PT J AU Dent, WRF Thi, WF Kamp, I Williams, JP Menard, F Andrews, S Ardila, D Aresu, G Augereau, JC Navascues, DBY Brittain, S Carmona, A Ciardi, D Danchi, W Donaldson, J Duchene, G Eiroa, C Fedele, D Grady, C de Gregorio-Molsalvo, I Howard, C Huelamo, N Krivov, A Lebreton, J Liseau, R Martin-Zaidi, C Mathews, G Meeus, G Mendigutia, I Montesinos, B Morales-Calderon, M Mora, A Nomura, H Pantin, E Pascucci, I Phillips, N Pinte, C Podio, L Ramsay, SK Riaz, B Riviere-Marichalar, P Roberge, A Sandell, G Solano, E Tilling, I Torrelles, JM Vandenbusche, B Vicente, S White, GJ Woitke, P AF Dent, W. R. F. Thi, W. F. Kamp, I. Williams, J. P. Menard, F. Andrews, S. Ardila, D. Aresu, G. Augereau, J. -C. Barrado y Navascues, D. Brittain, S. Carmona, A. Ciardi, D. Danchi, W. Donaldson, J. Duchene, G. Eiroa, C. Fedele, D. Grady, C. de Gregorio-Molsalvo, I. Howard, C. Huelamo, N. Krivov, A. Lebreton, J. Liseau, R. Martin-Zaidi, C. Mathews, G. Meeus, G. Mendigutia, I. Montesinos, B. Morales-Calderon, M. Mora, A. Nomura, H. Pantin, E. Pascucci, I. Phillips, N. Pinte, C. Podio, L. Ramsay, S. K. Riaz, B. Riviere-Marichalar, P. Roberge, A. Sandell, G. Solano, E. Tilling, I. Torrelles, J. M. Vandenbusche, B. Vicente, S. White, G. J. Woitke, P. TI GASPS-A Herschel Survey of Gas and Dust in Protoplanetary Disks: Summary and Initial Statistics SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID TW-HYDRAE ASSOCIATION; ETA-CHAMAELEONTIS CLUSTER; PICTORIS MOVING GROUP; HERBIG AE/BE SYSTEMS; TUCANA-HOROLOGIUM ASSOCIATION; SPITZER-MIPS OBSERVATIONS; AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE STARS; LOW-MASS PROTOSTARS; X-RAY-EMISSION AB We describe a large-scale far-infrared line and continuum survey of protoplanetary disk through to young debris disk systems carried out using the ACS instrument on the Herschel Space Observatory. This Open Time Key program, known as GASPS (Gas Survey of Protoplanetary Systems), targeted similar to 250 young stars in narrow wavelength regions covering the [OI] fine structure line at 63 mu m the brightest far-infrared line in such objects. A subset of the brightest targets were also surveyed in [OI]145 mu m, [CII] at 157 mu m, as well as several transitions of H2O and high-excitation CO lines at selected wavelengths between 78 and 180 mu m. Additionally, GASPS included continuum photometry at 70, 100 and 160 mu m, around the peak of the dust emission. The targets were SED Class II-III T Tauri stars and debris disks from seven nearby young associations, along with a comparable sample of isolated Herbig AeBe stars. The aim was to study the global gas and dust content in a wide sample of circumstellar disks, combining the results with models in a systematic way. In this overview paper we review the scientific aims, target selection and observing strategy of the program. We summarise some of the initial results, showing line identifications, listing the detections, and giving a first statistical study of line detectability. The [OI] line at 63 mu m was the brightest line seen in almost all objects, by a factor of similar to 10. Overall [OI]63 mu m detection rates were 49%, with 100% of HAeBe stars and 43% of T Tauri stars detected. A comparison with published disk dust masses (derived mainly from sub-mm continuum, assuming standard values of the mm mass opacity) shows a dust mass threshold for [OI] 63 mu m detection of similar to 10(-5) M-circle dot. Normalising to a distance of 140 pc, 84% of objects with dust masses >= 10(-5) M-circle dot can be detected in this line in the present survey; 32% of those of mass 10(-6)-10(-5) M-circle dot, and only a very small number of unusual objects with lower masses can be detected. This is consistent with models with a moderate UV excess and disk flaring. For a given disk mass, [OI] detectability is lower for M stars compared with earlier spectral types. Both the continuum and line emission was, in most systems, spatially and spectrally unresolved and centred on the star, suggesting that emission in most cases was from the disk. Approximately 10 objects showed resolved emission, most likely from outflows. In the GASPS sample, [OI] detection rates in T Tauri associations in the 0.3-4 Myr age range were similar to 50%. For each association in the 5-20 Myr age range, similar to 2 stars remain detectable in [OI]63 mu m, and no systems were detected in associations with age >20 Myr. Comparing with the total number of young stars in each association, and assuming a ISM-like gas/dust ratio, this indicates that similar to 18% of stars retain a gas-rich disk of total mass similar to 1 M-Jupiter for 1-4 Myr, 1-7% keep such disks for 5-10 Myr, but none are detected beyond 10-20 Myr. The brightest [OI] objects from GASPS were also observed in [OI]145 mu m, [CII]157 mu m and CO J = 18 - 17, with detection rates of 20-40%. Detection of the [CII] line was not correlated with disk mass, suggesting it arises more commonly from a compact remnant envelope. C1 [Dent, W. R. F.; de Gregorio-Molsalvo, I.; Phillips, N.; Podio, L.] ALMA SCO, Santiago, Chile. [Thi, W. F.; Kamp, I.; Aresu, G.; Vicente, S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Thi, W. F.; Menard, F.; Augereau, J. -C.; Carmona, A.; Duchene, G.; Lebreton, J.; Martin-Zaidi, C.; Pinte, C.] IPAG, UJF Grenoble 1, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Williams, J. P.; Mathews, G.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Andrews, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ardila, D.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Barrado y Navascues, D.; Huelamo, N.; Mendigutia, I.; Montesinos, B.; Morales-Calderon, M.; Riviere-Marichalar, P.; Solano, E.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, E-28691 Villanueva De La Canada, Spain. [Barrado y Navascues, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, E-04004 Almera, Spain. [Brittain, S.] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29634 USA. [Ciardi, D.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Danchi, W.; Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Donaldson, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Eiroa, C.; Meeus, G.] UAM Campus Cantoblanco, Fac Ciencias, Dep Fis, Madrid, Spain. [Fedele, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Grady, C.] Eureka Sci, Oakland, CA USA. [Howard, C.; Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Krivov, A.] Univ Jena, Inst Astrophys, Jena, Germany. [Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43900 Onsala, Sweden. [Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Nomura, H.] Kyoto Univ, Grad Sch Sci, Dept Astron, Kyoto 6068502, Japan. [Pantin, E.] Univ Paris Diderot, IRFU SAp, CNRS, CEA DSM,Lab AIM,CE Saclay, Paris, France. [Pascucci, I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Ramsay, S. K.] European So Observ, D-85748 Garching, Germany. [Riaz, B.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Tilling, I.] Univ Edinburgh, Royal Observ, Edinburgh, Midlothian, Scotland. [Torrelles, J. M.] Univ Barcelona, CSIC UB IEEC, Barcelona, Spain. [Vandenbusche, B.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, RALSpace, Didcot OX11 0NL, Oxon, England. [Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. RP Dent, WRF (reprint author), ALMA SCO, Alonso Cordova 3107, Santiago, Chile. RI Fedele, Davide/L-8688-2013; Roberge, Aki/D-2782-2012; Barrado Navascues, David/C-1439-2017; Solano, Enrique/C-2895-2017; Huelamo, Nuria/C-3042-2017; Montesinos, Benjamin/C-3493-2017; Morales-Calderon, Maria/C-8384-2017; OI Fedele, Davide/0000-0001-6156-0034; Roberge, Aki/0000-0002-2989-3725; Barrado Navascues, David/0000-0002-5971-9242; Huelamo, Nuria/0000-0002-2711-8143; Montesinos, Benjamin/0000-0002-7982-2095; Morales-Calderon, Maria/0000-0001-9526-9499; Torrelles, Jose Maria/0000-0002-6896-6085; Mendigutia, Ignacio/0000-0002-0233-5328; Ciardi, David/0000-0002-5741-3047 FU ANR [BLAN-0221, 0504-01, 0505-01]; European Commission's 7th Framework program [pERG06-GA-2009-256513]; CNES; PNPS of CNRS/INSU, France; EU FP7 [284405]; Scottish University physics Alliance fellowship; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX We wish to acknowledge the Herschel Helpdesk for their timely and useful responses. The Grenoble group thanks ANR (contracts BLAN-0221, 0504-01 and 0505-01), European Commission's 7th Framework program (contract pERG06-GA-2009-256513), CNES, and PNPS of CNRS/INSU, France for support. PW, IK, and WFT acknowledge funding from the EU FP7-2011 under Grant Agreement nr. 284405. WFT acknowledges a Scottish University physics Alliance fellowship (2006-2009).PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). NR 173 TC 41 Z9 42 U1 0 U2 10 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 MAY PY 2013 VL 125 IS 927 BP 477 EP 505 DI 10.1086/670826 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162CK UT WOS:000320241800001 ER PT J AU Han, ST Lee, JW Kang, J Oh, CS Byun, DY Je, DH Chung, MH Wi, SO Song, M Kang, YW Lee, SS Kim, SY Sasao, T Goldsmith, PF Wylde, R AF Han, Seog-Tae Lee, Jung-Won Kang, Jiman Oh, Chung-Sik Byun, Do-Young Je, Do-Heung Chung, Moon-Hee Wi, Seog-Oh Song, Minkyu Kang, Yong-Woo Lee, Sang-Sung Kim, Soo-Yeon Sasao, Tetsuo Goldsmith, Paul F. Wylde, Richard TI Korean VLBI Network Receiver Optics for Simultaneous Multifrequency Observation: Evaluation SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID PHASE COMPENSATION EXPERIMENTS; PAIRED ANTENNAS METHOD; RADIO TELESCOPES; 43 GHZ; MONITORS AB We have developed a new millimeter wave receiver system with input optics that support simultaneous observations in four bands of 22, 43, 86, and 129 GHz to facilitate calibrating tropospheric phase fluctuations for millimeter-wave VLBI observations. In order to make simultaneous observations in four bands pointing at the same position in sky, it is crucial that errors among the beams from any misalignments should be kept small. After doing the beam alignment in the laboratory, on-site test observations were carried out so as to evaluate the performance. The result is that the beam centers of the four bands with reference to the 86 GHz beam center were aligned within 2 '' over most of the elevation range of the Korean VLBI Network (KVN) 21 m telescope. Measured telescope aperture efficiencies including the multiband receiver optics are 65% at 22 GHz, 62% at 43 GHz, 57% at 86 GHz, and 38% at 129 GHz. Through this novel optics covering wide RF bandwidth effectively, we can simultaneously observe the SiO maser transitions at 43, 86, and 129 GHz and in addition the water maser line at 22 GHz. C1 [Han, Seog-Tae; Lee, Jung-Won; Kang, Jiman; Oh, Chung-Sik; Byun, Do-Young; Je, Do-Heung; Chung, Moon-Hee; Wi, Seog-Oh; Song, Minkyu; Kang, Yong-Woo; Lee, Sang-Sung] Korea Astron & Space Sci Inst, Taejon, South Korea. [Kim, Soo-Yeon; Sasao, Tetsuo] Korea Univ, Sch Elect Engn, Seoul, South Korea. [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Han, ST (reprint author), Korea Astron & Space Sci Inst, Taejon, South Korea. EM sthan@kasi.re.kr RI Goldsmith, Paul/H-3159-2016 NR 22 TC 19 Z9 19 U1 1 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 MAY PY 2013 VL 125 IS 927 BP 539 EP 547 DI 10.1086/671125 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162CK UT WOS:000320241800005 ER PT J AU Ellingson, SW Taylor, GB Craig, J Hartman, J Dowell, J Wolfe, CN Clarke, TE Hicks, BC Kassim, NE Ray, PS Rickard, LJ Schinzel, FK Weiler, KW AF Ellingson, S. W. Taylor, G. B. Craig, J. Hartman, J. Dowell, J. Wolfe, C. N. Clarke, T. E. Hicks, B. C. Kassim, N. E. Ray, P. S. Rickard, L. J. Schinzel, F. K. Weiler, K. W. TI The LWA1 Radio Telescope SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Antenna array; beamforming; radio astronomy ID ACTIVE ANTENNA; LOW-FREQUENCY; SYSTEM; ARRAY AB LWA1 is a new radio telescope operating in the frequency range 10-88 MHz, located in central New Mexico. The telescope consists of 258 pairs of dipole-type antennas whose outputs are individually digitized and formed into beams. Simultaneously, signals from all dipoles can be recorded using one of the instrument's "all dipoles" modes, facilitating all-sky imaging. Notable features of the instrument include high intrinsic sensitivity (approximate to 6 kJy zenith system equivalent flux density), large instantaneous bandwidth (up to 78 MHz), and four independently steerable beams utilizing digital "true time delay" beamforming. This paper summarizes the design of LWA1 and its performance as determined in commissioning experiments. We describe the method currently in use for array calibration, and report on measurements of sensitivity and beamwidth. C1 [Ellingson, S. W.; Wolfe, C. N.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. [Taylor, G. B.; Craig, J.; Dowell, J.; Rickard, L. J.; Schinzel, F. K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Hartman, J.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Clarke, T. E.; Hicks, B. C.; Kassim, N. E.; Ray, P. S.] USN, Res Lab, Washington, DC 20375 USA. [Weiler, K. W.] Computat Phys Inc, Springfield, VA 22151 USA. RP Ellingson, SW (reprint author), Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. EM ellingson@vt.edu; gbtaylor@unm.edu; namir.kassim@nrl.navy.mil OI Ray, Paul/0000-0002-5297-5278 FU U.S. Office of Naval Research [N00014-07-C-0147]; National Science Foundation [AST-1139963, AST-1139974]; Naval Research Laboratory; National Radio Astronomy Observatory FX The authors acknowledge the helpful comments of M. Davis. Construction of LWA1 has been supported by the U.S. Office of Naval Research under Contract N00014-07-C-0147. Support for operations and continuing development of LWA1 is provided by the National Science Foundation under Grant AST-1139963 and AST-1139974. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 base funding. The authors acknowledge the support of the National Radio Astronomy Observatory. NR 23 TC 42 Z9 42 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD MAY PY 2013 VL 61 IS 5 BP 2540 EP 2549 DI 10.1109/TAP.2013.2242826 PG 10 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 157BP UT WOS:000319870700022 ER PT J AU Cliff, SE Elmiligui, AA Campbell, RL Thomas, SD AF Cliff, Susan E. Elmiligui, Alaa A. Campbell, Richard L. Thomas, Scott D. TI Refined Tetrahedral Meshes with Mach Cone Aligned Prisms for Sonic Boom Analysis SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 29th AIAA Applied Aerodynamics Conference CY JUN 27-30, 2011 CL Honolulu, HI SP AIAA ID GENERATION AB A tetrahedral mesh generation method for acquiring accurate sonic boom pressure signatures several body lengths from an aircraft model has been developed. The method serves as a tool for aerodynamicists to efficiently create useful meshes for sonic boom analysis. The procedure includes generating a refined near-field grid with a cylindrically shaped boundary that encompasses the model just beyond its surface and a prismatic mesh from the cylindrical boundary to the far field. Projecting the boundary in the radial direction and forming prisms. between neighboring layer faces creates the prism mesh. Each prism is subdivided into three tetrahedra resulting in a mesh comprised entirely of tetrahedral cells. The prism structure permits radial stretching and mesh alignment with the Mach cone around the aircraft model for accurate on- and offtrack signatures. Computational results for four models compared with experimental data validate this methodology. C1 [Cliff, Susan E.] NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Moffett Field, CA 94035 USA. [Elmiligui, Alaa A.; Campbell, Richard L.] NASA, Langley Res Ctr, Hampton, VA 23669 USA. [Thomas, Scott D.] Dell Serv Fed Govt, Moffett Field, CA 94035 USA. RP Cliff, SE (reprint author), NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, M-S 258-2, Moffett Field, CA 94035 USA. NR 44 TC 0 Z9 0 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD MAY-JUN PY 2013 VL 50 IS 3 BP 778 EP 790 DI 10.2514/1.C031943 PG 13 WC Engineering, Aerospace SC Engineering GA 159VQ UT WOS:000320075800010 ER PT J AU Khoshakhlagh, A Hoglund, L Ting, DZ Hill, CJ Keo, SA Soibel, A Nguyen, J Gunapala, SD AF Khoshakhlagh, Arezou Hoeglund, Linda Ting, David Z. Hill, Cory J. Keo, Sam A. Soibel, Alexander Nguyen, Jean Gunapala, Sarath D. TI High performance long-wave type-II superlattice infrared detectors SO JOURNAL OF VACUUM SCIENCE & TECHNOLOGY B LA English DT Article AB The authors report on growth, material characterization, and device performance of infrared photodetectors based on type II InAs/GaSb superlattices using the complementary barrier infrared detector (CBIRD) design. In this paper, control steps for improvement of material quality in terms of surface, structural, and optical properties of infrared detectors grown at Jet Propulsion Laboratory are described. For a specific CBIRD studied, these quality control steps indicate high structural and optical quality of the grown material. Furthermore, single-element detector from the optimized growth conditions exhibit dark current density less than 1 x 10(-5) A/cm(2) at applied biases up to V-b = 0.36 V (T = 77 K), so this material can be utilized for focal plane arrays development. (C) 2013 American Vacuum Society. C1 [Khoshakhlagh, Arezou; Hoeglund, Linda; Ting, David Z.; Hill, Cory J.; Keo, Sam A.; Soibel, Alexander; Nguyen, Jean; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Ctr Infrared Sensors, Pasadena, CA 91109 USA. RP Khoshakhlagh, A (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Sensors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Arezou.Khoshakhlagh@jpl.nasa.gov RI Soibel, Alexander/A-1313-2007 NR 15 TC 5 Z9 5 U1 1 U2 30 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 MAY PY 2013 VL 31 IS 3 AR 03C122 DI 10.1116/1.4798485 PG 4 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA 160PB UT WOS:000320130500022 ER PT J AU Filippova, SN Surgucheva, NA Kulikov, EE Sorokin, VV Akimov, VN Bej, AK McKay, C Andersen, D Galchenko, VF AF Filippova, S. N. Surgucheva, N. A. Kulikov, E. E. Sorokin, V. V. Akimov, V. N. Bej, A. K. McKay, C. Andersen, D. Galchenko, V. F. TI Detection of phage infection in the bacterial population of Lake Untersee (Antarctica) SO MICROBIOLOGY LA English DT Article ID DRONNING MAUD LAND; EAST ANTARCTICA; BACTERIOPHAGE; METHANE C1 [Filippova, S. N.; Surgucheva, N. A.; Kulikov, E. E.; Sorokin, V. V.; Akimov, V. N.; Galchenko, V. F.] Russian Acad Sci, Winogradsky Inst Microbiol, Moscow 117312, Russia. [Akimov, V. N.] Russian Acad Sci, Skryabin Inst Biochem & Physiol Microorganisms, Pushchino 142290, Moscow Oblast, Russia. [Bej, A. K.] Univ Alabama Birmingham, Birmingham, AL 35294 USA. [McKay, C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Andersen, D.] SETI Inst, Mountain View, CA 94043 USA. RP Filippova, SN (reprint author), Russian Acad Sci, Winogradsky Inst Microbiol, Pr 60 Letiya Oktyabrya 7,K1, Moscow 117312, Russia. EM svfilipova@mail.ru; valgalch@inmi.host.ru RI Filippova, Svetlana/F-3277-2014 FU Russian Foundation for Basic Research [11-05-00-961-a] FX This work was supported by the Russian Foundation for Basic Research, project no. 11-05-00-961-a. NR 19 TC 1 Z9 2 U1 1 U2 5 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0026-2617 J9 MICROBIOLOGY+ JI Microbiology PD MAY PY 2013 VL 82 IS 3 BP 383 EP 386 DI 10.1134/S0026261713030041 PG 4 WC Microbiology SC Microbiology GA 163EL UT WOS:000320318500015 ER PT J AU Guhathakurta, M Phillips, T AF Guhathakurta, Madhulika Phillips, Tony TI The Solar Cycle Turned Sideways SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE solar cycle; space weather; impacts C1 [Guhathakurta, Madhulika] NASAs Headquarters, Living Star Program, Washington, DC USA. [Phillips, Tony] NASA Headquarters, Sci NASA, Washington, DC USA. RP Guhathakurta, M (reprint author), NASAs Headquarters, Living Star Program, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1539-4956 J9 SPACE WEATHER JI Space Weather PD MAY PY 2013 VL 11 IS 5 BP 212 EP 213 DI 10.1002/swe.20039 PG 2 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 166MR UT WOS:000320559400003 ER PT J AU Savani, NP Vourlidas, A Pulkkinen, A Nieves-Chinchilla, T Lavraud, B Owens, MJ AF Savani, N. P. Vourlidas, A. Pulkkinen, A. Nieves-Chinchilla, T. Lavraud, B. Owens, M. J. TI Tracking the momentum flux of a CME and quantifying its influence on geomagnetically induced currents at Earth SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE coronal mass ejections; geomagnetically induced currents ID CORONAL MASS EJECTIONS; GREAT MAGNETIC STORMS; SOLAR-WIND; RING CURRENT; 1 AU; OBSERVATIONAL EVIDENCE; TECHNOLOGICAL SYSTEMS; MHD SIMULATIONS; STEREO MISSION; FIELD AB We investigate a coronal mass ejection (CME) propagating toward Earth on 29 March 2011. This event is specifically chosen for its predominately northward directed magnetic field, so that the influence from the momentum flux onto Earth can be isolated. We focus our study on understanding how a small Earth-directed segment propagates. Mass images are created from the white-light cameras onboard STEREO which are also converted into mass height-time maps (mass J-maps). The mass tracks on these J-maps correspond to the sheath region between the CME and its associated shock front as detected by in situ measurements at L1. A time series of mass measurements from the STEREO COR-2A instrument is made along the Earth propagation direction. Qualitatively, this mass time series shows a remarkable resemblance to the L1 in situ density series. The in situ measurements are used as inputs into a three-dimensional (3-D) magnetospheric space weather simulation from the Community Coordinated Modeling Center. These simulations display a sudden compression of the magnetosphere from the large momentum flux at the leading edge of the CME, and predictions are made for the time derivative of the magnetic field (dB/dt) on the ground. The predicted dB/dt values were then compared with the observations from specific equatorially located ground stations and showed notable similarity. This study of the momentum of a CME from the Sun down to its influence on magnetic ground stations on Earth is presented as a preliminary proof of concept, such that future attempts may try to use remote sensing to create density and velocity time series as inputs to magnetospheric simulations. C1 [Savani, N. P.] UCAR, Boulder, CO USA. [Savani, N. P.; Pulkkinen, A.; Nieves-Chinchilla, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vourlidas, A.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Pulkkinen, A.; Nieves-Chinchilla, T.] Catholic Univ Amer, IACS, Washington, DC 20064 USA. [Lavraud, B.] Univ Toulouse UPS, Inst Rech Astrophys & Planetol, Toulouse, France. [Lavraud, B.] CNRS, UMR 5277, Toulouse, France. [Owens, M. J.] Univ Reading, Space Environm Phys Grp, Reading, Berks, England. RP Savani, NP (reprint author), Naval Res Lab, Solar Phys Branch, 4555 Overlook Ave SW, Washington, DC 20375 USA. EM neel.savani02@imperial.ac.uk RI Savani, Neel/G-4066-2014; Vourlidas, Angelos/C-8231-2009; Owens, Mathew/B-3006-2010; Nieves-Chinchilla, Teresa/F-3482-2016 OI Savani, Neel/0000-0002-1916-7877; Vourlidas, Angelos/0000-0002-8164-5948; Owens, Mathew/0000-0003-2061-2453; Nieves-Chinchilla, Teresa/0000-0003-0565-4890 FU NASA; NASA [S-136361-Y] FX N.P.S. thanks Neil Sheeley and Adam Szabo for their collaborative assistance. This research was also supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs and hosted by the Naval Research Laboratory. AV is supported by NASA contract S-136361-Y. The global MHD simulations used in this work were carried out at the Community Coordinated Modeling Center (CCMC) operated at NASA Goddard Space Flight Center. The authors wish to acknowledge Lutz Rastaetter, David Berrios, and the rest of the CCMC staff for their generous support throughout the work discussed in the paper. The results presented in this paper rely on the data collected at Vassouras, Kakadu, and Kanoya. We thank Observatorio Nacional, Geoscience Australia, and Japan Meteorological Agency for supporting its operation and International Real-time Magnetic Observatory Network (INTERMAGNET) for promoting high standards of magnetic observatory practice (www.intermagnet.org). NR 114 TC 7 Z9 7 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD MAY PY 2013 VL 11 IS 5 BP 245 EP 261 DI 10.1002/swe.20038 PG 17 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 166MR UT WOS:000320559400008 ER PT J AU Honkonen, I Rastatter, L Grocott, A Pulkkinen, A Palmroth, M Raeder, J Ridley, AJ Wiltberger, M AF Honkonen, I. Rastaetter, L. Grocott, A. Pulkkinen, A. Palmroth, M. Raeder, J. Ridley, A. J. Wiltberger, M. TI On the performance of global magnetohydrodynamic models in the Earth's magnetosphere SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE global MHD; Earth's magnetosphere; validation ID HIGH-LATITUDE CONVECTION; HF RADAR OBSERVATIONS; MAGNETIC-FIELD; SIMULATION; COMMUNITY; SCHEME AB We study the performance of four magnetohydrodynamic models (BATS-R-US, GUMICS, LFM, OpenGGCM) in the Earth's magnetosphere. Using the Community Coordinated Modeling Center's Run-on-Request system, we compare model predictions with magnetic field measurements of the Cluster, Geotail and Wind spacecraft during a multiple substorm event. We also compare model cross polar cap potential results to those obtained from the Super Dual Auroral Radar Network (SuperDARN) and the model magnetopause standoff distances to an empirical magnetopause model. The correlation coefficient (CC) and prediction efficiency (PE) metrics are used to objectively evaluate model performance quantitatively. For all four models, the best performance outside geosynchronous orbit is found on the dayside. Generally, the performance of models decreases steadily downstream from the Earth. On the dayside most CCs are above 0.5 with CCs for Bx and Bz close to 0.9 for three out of four models. In the magnetotail at a distance of about -130 Earth radii from Earth, the prediction efficiency of all models is below that of using an average value for the prediction with the exception of Bz. Bx is most often best predicted and correlated both on the dayside and the nightside close to the Earth whereas in the far tail the CC and PE for Bz are substantially higher than other components in all models. We also find that increasing the resolution or coupling an additional physics module does not automatically increase the model performance in the magnetosphere. C1 [Honkonen, I.; Palmroth, M.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Honkonen, I.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Rastaetter, L.; Pulkkinen, A.] NASA, Goddard Space Flight Ctr, Commun Coordinated Modeling Ctr, Greenbelt, MD 20771 USA. [Grocott, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Pulkkinen, A.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Raeder, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Raeder, J.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Ridley, A. J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Honkonen, I (reprint author), Finnish Meteorol Inst, PL 503, FIN-00101 Helsinki, Finland. EM ilja.honkonen@fmi.fi RI Wiltberger, Michael/B-8781-2008; Rastaetter, Lutz/D-4715-2012; Ridley, Aaron/F-3943-2011 OI Wiltberger, Michael/0000-0002-4844-3148; Rastaetter, Lutz/0000-0002-7343-4147; Ridley, Aaron/0000-0001-6933-8534 FU European Research Council under the European Community [200141-QuESpace]; Academy of Finland [218165]; NERC [NE/G019665/1]; National Science Foundation FX This work is a part of the project 200141-QuESpace, funded by the European Research Council under the European Community's seventh framework programme. The work of I.H. and M.P. is supported by project 218165 of the Academy of Finland. A.G. is supported by NERC Grant NE/G019665/1. The National Center for Atmospheric Research is supported by the National Science Foundation. We thank the rest of the CCMC staff for providing a valuable service, the Cluster Active Archive, Coordinated Data Analysis Web and the instrument teams and PIs of Geotail MGF, Wind MFI, Cluster FGM, and ACE MAG and SWEPAM (S. Kokubun, R. Lepping, A. Balogh, N.F. Ness, D.J. McComas, respectively) for providing the spacecraft data used in this study. We also thank the World Data Center for Geomagnetism for the Kyoto AE and Dst index services and the anonymous referee for insightful comments. I.H. thanks C. Anekallu for insightful discussions. NR 34 TC 7 Z9 7 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1539-4956 J9 SPACE WEATHER JI Space Weather PD MAY PY 2013 VL 11 IS 5 BP 313 EP 326 DI 10.1002/swe.20055 PG 14 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 166MR UT WOS:000320559400014 ER PT J AU Cavalie, T Feuchtgruber, H Lellouch, E de Val-Borro, M Jarchow, C Moreno, R Hartogh, P Orton, G Greathouse, TK Billebaud, F Dobrijevic, M Lara, LM Gonzalez, A Sagawa, H AF Cavalie, T. Feuchtgruber, H. Lellouch, E. de Val-Borro, M. Jarchow, C. Moreno, R. Hartogh, P. Orton, G. Greathouse, T. K. Billebaud, F. Dobrijevic, M. Lara, L. M. Gonzalez, A. Sagawa, H. TI Spatial distribution of water in the stratosphere of Jupiter from Herschel HIFI and PACS observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: individual: Jupiter; planets and satellites: atmospheres; submillimeter: planetary systems ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; PROBE MASS-SPECTROMETER; ODIN SPACE TELESCOPE; CARBON-MONOXIDE; COMET SHOEMAKER-LEVY-9; NEPTUNES STRATOSPHERE; UPPER-ATMOSPHERE; SOLAR-SYSTEM; VAPOR; CO AB Context. In the past 15 years, several studies suggested that water in the stratosphere of Jupiter originated from the Shoemaker-Levy 9 (SL9) comet impacts in July 1994, but a direct proof was missing. Only a very sensitive instrument observing with high spectral/spatial resolution can help to solve this problem. This is the case of the Herschel Space Observatory, which is the first telescope capable of mapping water in Jupiter's stratosphere. Aims. We observed the spatial distribution of the water emission in Jupiter's stratosphere with the Heterodyne Instrument for the Far Infrared (HIFI) and the Photodetector Array Camera and Spectrometer (PACS) onboard Herschel to constrain its origin. In parallel, we monitored Jupiter's stratospheric temperature with the NASA Infrared Telescope Facility (IRTF) to separate temperature from water variability. Methods. We obtained a 25-point map of the 1669.9 GHz water line with HIFI in July 2010 and several maps with PACS in October 2009 and December 2010. The 2010 PACS map is a 400-point raster of the water 66.4 mu m emission. Additionally, we mapped the methane nu(4) band emission to constrain the stratospheric temperature in Jupiter in the same periods with the IRTF. Results. Water is found to be restricted to pressures lower than 2mbar. Its column density decreases by a factor of 2-3 between southern and northern latitudes, consistently between the HIFI and the PACS 66.4 mu m maps. We infer that an emission maximum seen around 15 degrees S is caused by a warm stratospheric belt detected in the IRTF data. Conclusions. Latitudinal temperature variability cannot explain the global north-south asymmetry in the water maps. From the latitudinal and vertical distributions of water in Jupiter's stratosphere, we rule out interplanetary dust particles as its main source. Furthermore, we demonstrate that Jupiter's stratospheric water was delivered by the SL9 comet and that more than 95% of the observed water comes from the comet according to our models. C1 [Cavalie, T.; Billebaud, F.; Dobrijevic, M.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Cavalie, T.; Billebaud, F.; Dobrijevic, M.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Feuchtgruber, H.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Lellouch, E.; Moreno, R.] Univ Paris Diderot, LESIA Observ Paris, CNRS, Univ Paris 06, F-92195 Meudon, France. [de Val-Borro, M.; Jarchow, C.; Hartogh, P.; Gonzalez, A.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [de Val-Borro, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Orton, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Greathouse, T. K.] SW Res Inst, San Antonio, TX 78228 USA. [Lara, L. M.; Gonzalez, A.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Sagawa, H.] Natl Inst Informat & Commun Technol, Koganei, Tokyo 1848795, Japan. RP Cavalie, T (reprint author), Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. EM cavalie@obs.u-bordeaux1.fr FU Centre National d'Etudes Spatiales (CNES); Special Priority Program 1488 of the German Science Foundation; National Aeronautics and Space Administration; NASA PAST grant [NNX08AW33G]; National Aeronautics and Space Administration [NNX-08AE38A]; Programme National de Planetologie (PNP) of the Institut National des Sciences de l'Univers (INSU); CEA; CNES; CNRS (France); ASI (Italy); DLR (Germany); ESA; [NSF AST-1108686]; [NASA NNX12AH91H] FX T. Cavalie wishes to thank J. Brillet for providing him with his baseline ripple removal tool for the purposes of this work. T. Cavalie acknowledges funding from the Centre National d'Etudes Spatiales (CNES). M. de Val-Borro acknowledges support from the Special Priority Program 1488 of the German Science Foundation, and grants NSF AST-1108686 and NASA NNX12AH91H. G. Orton acknowledges funding from the National Aeronautics and Space Administration to the Jet Propulsion Laboratory, California Institute of Technology. T. Greathouse acknowledges funding from NASA PAST grant NNX08AW33G and was supported as a Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. F. Billebaud wishes to thank the Programme National de Planetologie (PNP) of the Institut National des Sciences de l'Univers (INSU) for pluriannual funding on this project. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain). Data presented in this paper were analyzed using HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. This development has been supported by national funding agencies: CEA, CNES, CNRS (France); ASI (Italy); DLR (Germany). Additional funding support for some instrument activities has been provided by ESA. We are grateful to an anonymous referee for the constructive comments about this manuscript. NR 57 TC 10 Z9 10 U1 1 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR A21 DI 10.1051/0004-6361/201220797 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700021 ER PT J AU Delabrouille, J Betoule, M Melin, JB Miville-Deschenes, MA Gonzalez-Nuevo, J Le Jeune, M Castex, G de Zotti, G Basak, S Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Bernard, JP Bouchet, FR Clements, DL da Silva, A Dickinson, C Dodu, F Dolag, K Elsner, F Fauvet, L Fay, G Giardino, G Leach, S Lesgourgues, J Liguori, M Macias-Perez, JF Massardi, M Matarrese, S Mazzotta, P Montier, L Mottet, S Paladini, R Partridge, B Piffaretti, R Prezeau, G Prunet, S Ricciardi, S Roman, M Schaefer, B Toffolatti, L AF Delabrouille, J. Betoule, M. Melin, J. -B. Miville-Deschenes, M. -A. Gonzalez-Nuevo, J. Le Jeune, M. Castex, G. de Zotti, G. Basak, S. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Bernard, J. -P. Bouchet, F. R. Clements, D. L. da Silva, A. Dickinson, C. Dodu, F. Dolag, K. Elsner, F. Fauvet, L. Fay, G. Giardino, G. Leach, S. Lesgourgues, J. Liguori, M. Macias-Perez, J. F. Massardi, M. Matarrese, S. Mazzotta, P. Montier, L. Mottet, S. Paladini, R. Partridge, B. Piffaretti, R. Prezeau, G. Prunet, S. Ricciardi, S. Roman, M. Schaefer, B. Toffolatti, L. TI The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: miscellaneous; radio continuum: general; submillimeter: general; cosmic background radiation; ISM: general; galaxies: general ID MICROWAVE-ANISOTROPY-PROBE; SOUTH-POLE TELESCOPE; ATACAMA COSMOLOGY TELESCOPE; HIGH GALACTIC LATITUDES; INTERNAL LINEAR COMBINATION; NRAO PMN SURVEYS; H-II REGIONS; ASTROPHYSICAL DUST EMISSION; COEVAL OBSERVATIONS PROJECT; BLIND COMPONENT SEPARATION AB We present the Planck Sky Model (PSM), a parametric model for generating all-sky, few arcminute resolution maps of sky emission at submillimetre to centimetre wavelengths, in both intensity and polarisation. Several options are implemented to model the cosmic microwave background, Galactic diffuse emission (synchrotron, free-free, thermal and spinning dust, CO lines), Galactic HII regions, extragalactic radio sources, dusty galaxies, and thermal and kinetic Sunyaev-Zeldovich signals from clusters of galaxies. Each component is simulated by means of educated interpolations/extrapolations of data sets available at the time of the launch of the Planck mission, complemented by state-of-the-art models of the emission. Distinctive features of the simulations are spatially varying spectral properties of synchrotron and dust; different spectral parameters for each point source; modelling of the clustering properties of extragalactic sources and of the power spectrum of fluctuations in the cosmic infrared background. The PSM enables the production of random realisations of the sky emission, constrained to match observational data within their uncertainties. It is implemented in a software package that is regularly updated with incoming information from observations. The model is expected to serve as a useful tool for optimising planned microwave and sub-millimetre surveys and testing data processing and analysis pipelines. It is, in particular, used to develop and validate data analysis pipelines within the Planck collaboration. A version of the software that can be used for simulating the observations for a variety of experiments is made available on a dedicated website. C1 [Delabrouille, J.; Le Jeune, M.; Castex, G.; Basak, S.; Dodu, F.; Fay, G.; Roman, M.] Univ Paris 07, CNRS, UMR7164, Lab APC, F-75013 Paris, France. [Betoule, M.] LPNHE, F-75252 Paris 05, France. [Betoule, M.] PCCP, F-75205 Paris, France. [Melin, J. -B.; Piffaretti, R.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Miville-Deschenes, M. -A.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3HB, Canada. [Gonzalez-Nuevo, J.; de Zotti, G.; Baccigalupi, C.; Leach, S.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [de Zotti, G.; Massardi, M.] Osserv Astron Padova, INAF, Padua, Italy. [Ashdown, M.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Ashdown, M.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Banday, A. J.; Bernard, J. -P.; Montier, L.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Aumont, J.; Baccigalupi, C.; Montier, L.] CNRS, IRAP9, F-31028 Toulouse 4, France. [Bouchet, F. R.; Elsner, F.; Liguori, M.; Mottet, S.; Prunet, S.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, Paris, France. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [da Silva, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Dickinson, C.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Dolag, K.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Fauvet, L.; Giardino, G.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Fay, G.] Ecole Cent Paris, Lab MAS, F-92295 Chatenay Malabry, France. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, Inst Theorie Phenomenes Phys, CH-1015 Lausanne, Switzerland. [Lesgourgues, J.] CERN, Div Theory, CH-1211 Geneva 23, Switzerland. [Lesgourgues, J.] Univ Savoie, CNRS, LAPTh, F-74941 Annecy Le Vieux, France. [Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Macias-Perez, J. F.] Univ Grenoble 1, CNRS, IN2P3, Inst Natl Polytech Grenoble,LPSC, F-38026 Grenoble, France. [Massardi, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Paladini, R.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Prezeau, G.] CALTECH, Pasadena, CA 91125 USA. [Prezeau, G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Ricciardi, S.] INAF IASF, I-40129 Bologna, Italy. [Schaefer, B.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. RP Delabrouille, J (reprint author), Univ Paris 07, CNRS, UMR7164, Lab APC, 10 Rue A Domon & L Duquet, F-75013 Paris, France. EM delabrouille@apc.univ-paris7.fr RI Da Silva, Antonio/A-2693-2010; Bouchet, Francois/B-5202-2014; Toffolatti, Luigi/K-5070-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Mazzotta, Pasquale/B-1225-2016; OI Da Silva, Antonio/0000-0002-6385-1609; Toffolatti, Luigi/0000-0003-2645-7386; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Mazzotta, Pasquale/0000-0002-5411-1748; De Zotti, Gianfranco/0000-0003-2868-2595; Matarrese, Sabino/0000-0002-2573-1243; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (Spain); JA (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU); "Physique des deux Infinis" (P2I) Consortium; STFC Advanced Fellowship; ERC IRG grant FX We wish to thank our colleagues from the Planck Collaboration, and in particular members of the component separation working group (WG2), for useful suggestions and discussions, as well as for beta-testing the successive versions of the software. We thank Karim Benabed, Frederic Guilloux, Frode Hansen and Benjamin Wandelt for useful discussions concerning some of the CMB models. Francois Boulanger, Rodney Davies and Francois-Xavier Desert have provided expertise for developing the model of Galactic emission used in this work. We thank Francesca Perrotta, Grazia Umana and Stephen Serjeant for useful discussions concerning the point source model, Benjamin Walter for his help in the editing of the present paper, Hans-Kristian Eriksen, Torsten Ensslin, Andrew Jaffe, Lloyd Knox and Douglas Scott for useful comments on the PSM paper draft, and Pei Yu for her help setting-up a data repository for PSM activities. This work has been developed largely within the Planck Collaboration. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at (http://www.rssd.esa.int/index.php?project=PLANCK\&page=Planck_Collabora tion). The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). SB has been supported by a postdoctoral grant from the "Physique des deux Infinis" (P2I) Consortium. CD acknowledges an STFC Advanced Fellowship and an ERC IRG grant under the FP7. NR 262 TC 67 Z9 67 U1 2 U2 13 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR UNSP A96 DI 10.1051/0004-6361/201220019 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700096 ER PT J AU Ferrigno, C Farinelli, R Bozzo, E Pottschmidt, K Klochkov, D Kretschmar, P AF Ferrigno, C. Farinelli, R. Bozzo, E. Pottschmidt, K. Klochkov, D. Kretschmar, P. TI RX J0440.9+4431: a persistent Be/X-ray binary in outburst SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; X-rays: individuals: RX J0440.9+4431; stars: neutron ID THREADED ACCRETION DISK; XMM-NEWTON OBSERVATION; BULK COMPTONIZATION; SPECTRAL FORMATION; NEUTRON-STARS; PULSARS; DISCOVERY; MISSION; ABSORPTION; MODELS AB The persistent Be/X-ray binary RXJ0440.9+4431 flared in 2010 and 2011 and has been followed by various X-ray facilities (Swift, RXTE, XMM-Newton, and INTEGRAL). We studied the source timing and spectral properties as a function of its X-ray luminosity to investigate the transition from normal to flaring activity and the dynamical properties of the system. We have determined the orbital period from the long-term Swift/BAT light curve, but our determinations of the spin-period are not precise enough to constrain any orbital solution. The source spectrum can always be described by a bulk-motion Comptonization model of black body seed photons attenuated by a moderate photoelectric absorption. At the highest luminosity, we measured a curvature of the spectrum, which we attribute to a significant contribution of the radiation pressure in the accretion process. This allows us to estimate that the transition from a bulk-motion-dominated flow to a radiatively dominated one happens at a luminosity of similar to 2 x 10(36) erg s(-1). The luminosity dependency of the size of the black body emission region is found to be r(BB) proportional to L-X(0.39+/-0.02). This suggests that either matter accreting onto the neutron star hosted in RXJ0440.9+4431 penetrates through closed magnetic field lines at the border of the compact object magnetosphere or that the structure of the neutron star magnetic field is more complicated than a simple dipole close to the surface. C1 [Ferrigno, C.; Bozzo, E.] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Farinelli, R.] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. [Pottschmidt, K.] CRESST, Baltimore, MD 21250 USA. [Pottschmidt, K.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Klochkov, D.] Univ Tubingen, IAAT, Abt Astron, D-72076 Tubingen, Germany. [Kretschmar, P.] ISOC, ESAC, Madrid, Spain. RP Ferrigno, C (reprint author), Univ Geneva, ISDC Data Ctr Astrophys, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. EM Carlo.Ferrigno@unige.ch OI Kretschmar, Peter/0000-0001-9840-2048 NR 51 TC 5 Z9 5 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR UNSP A103 DI 10.1051/0004-6361/201321053 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700103 ER PT J AU Grafe, C Wolf, S Guilloteau, S Dutrey, A Stapelfeldt, KR Pontoppidan, KM Sauter, J AF Graefe, C. Wolf, S. Guilloteau, S. Dutrey, A. Stapelfeldt, K. R. Pontoppidan, K. M. Sauter, J. TI Vertical settling and radial segregation of large dust grains in the circumstellar disk of the Butterfly Star SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; stars: pre-main sequence; stars: individual: IRAS 04302+2247; circumstellar matter; planets and satellites: formation; radiative transfer ID SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; T-TAURI STARS; PROTOPLANETARY DISKS; GIANT PLANETS; PROTOSTELLAR DISKS; OLIGARCHIC GROWTH; EVOLUTION; PLANETESIMALS; MIGRATION AB Context. Circumstellar disks are considered to be the environment for the formation of planets. The growth of dust grains in these disks is the first step in the core accretion-gas capture planet formation scenario. Indicators and evidence of disk evolution can be traced in spatially resolved images and the spectral energy distribution (SED) of these objects. Aims. We develop a model for the dust phase of the edge-on oriented circumstellar disk of the Butterfly Star which allows one to fit observed multi-wavelength images and the SED simultaneously. Methods. Our model is based on spatially resolved high angular resolution observations at 1.3 mm, 894 mu m, 2.07 mu m, 1.87 mu m, 1.60 mu m, and 1.13 mu m and an extensively covered SED ranging from 12 mu m to 2.7 mm, including a detailed spectrum obtained with the Spitzer Space Telescope in the range from 12 mu m to 38 mu m. A parameter study based on a grid search method involving the detailed analysis of every parameter was performed to constrain the disk parameters and find the best-fit model for the independent observations. The individual observations were modeled simultaneously, using our continuum radiative transfer code. Results. We derived a model that is capable of reproducing all of the observations of the disk at the same time. We find quantitative evidence for grain growth up to similar to 100 mu m-sized particles, vertical settling of larger dust grains toward the disk midplane, and radial segregation of the latter toward the central star. Within our best-fit model the large grains have a distribution with a scale height of 3.7 AU at 100 AU and a radial extent of 175 AU compared to a hydrostatic scale height of 6.9 AU at 100 AU and an outer disk radius of 300 AU. Our results are consistent with current theoretical models for the evolution of circumstellar disks and the early stages of planet formation. C1 [Graefe, C.; Wolf, S.; Sauter, J.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24118 Kiel, Germany. [Guilloteau, S.; Dutrey, A.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Guilloteau, S.; Dutrey, A.] LAB, CNRS, UMR 5804, F-33270 Floirac, France. [Stapelfeldt, K. R.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pontoppidan, K. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Grafe, C (reprint author), Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24118 Kiel, Germany. EM cgraefe@astrophysik.uni-kiel.de FU DFG through the research group 759 [WO 857/4-2, WO 857/12-1] FX This work is supported by the DFG through the research group 759 "The Formation of Planets: The Critical First Growth Phase" (WO 857/4-2) and project WO 857/12-1. We are grateful to the anonymous referee for providing useful suggestions that greatly improved this paper. NR 90 TC 16 Z9 16 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR UNSP A69 DI 10.1051/0004-6361/201220720 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700069 ER PT J AU Lebouteiller, V Heap, S Hubeny, I Kunth, D AF Lebouteiller, V. Heap, S. Hubeny, I. Kunth, D. TI Chemical enrichment and physical conditions in I Zw 18 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: abundances; HII regions; galaxies: individual: I Zw 18; galaxies: ISM; galaxies: star formation; galaxies: evolution ID COMPACT DWARF GALAXIES; HUBBLE-SPACE-TELESCOPE; LY-ALPHA SYSTEMS; SPECTROSCOPIC-EXPLORER OBSERVATIONS; BLANKETED MODEL ATMOSPHERES; TRIGGERED STAR-FORMATION; DIGITAL SKY SURVEY; POLYCYCLIC AROMATIC-HYDROCARBONS; DIFFUSE INTERSTELLAR-MEDIUM; GIANT MOLECULAR CLOUDS AB Context. Low-metallicity star-forming dwarf galaxies are prime targets to understand the chemical enrichment of the interstellar medium. The H I region contains the bulk of the mass in blue compact dwarfs, and it provides important constraints on the dispersal and mixing of heavy elements released by successive star-formation episodes. The metallicity of the H I region is also a critical parameter to investigate the future star-formation history, as metals provide most of the gas cooling that will facilitate and sustain star formation. Aims. Our primary objective is to study the enrichment of the H I region and the interplay between star-formation history and metallicity evolution. Our secondary objective is to constrain the spatial-and time-scales over which the H I and H I I regions are enriched, and the mass range of stars responsible for the heavy element production. Finally, we aim to examine the gas heating and cooling mechanisms in the H I region. Methods. We observed the most metal-poor star-forming galaxy in the Local Universe, I Zw 18, with the Cosmic Origin Spectrograph onboard Hubble. The abundances in the neutral gas are derived from far-ultraviolet absorption-lines (H I, C II, C II*, N I, O I, ... ) and are compared to the abundances in the H II region. Models are constructed to calculate the ionization structure and the thermal processes. We investigate the gas cooling in the H I region through physical diagnostics drawn from the fine-structure level of C+. Results. We find that H I region abundances are lower by a factor of similar to 2 as compared to the H II region. There is no differential depletion on dust between the H I and H II region. Using sulfur as a metallicity tracer, we calculate a metallicity of 1/46 Z(circle dot) (vs. 1/31 Z(circle dot) in the H II region). From the study of the C/O, [O/Fe], and N/O abundance ratios, we propose that C, N, O, and Fe are mainly produced in massive stars. We argue that the H I envelope may contain pockets of pristine gas with a metallicity essentially null. Finally, we derive the physical conditions in the H I region by investigating the C II* absorption line. The cooling rate derived from C II* is consistent with collisions with H-0 atoms in the diffuse neutral gas. We calculate the star-formation rate from the C II* cooling rate assuming that photoelectric effect on dust is the dominant gas heating mechanism. Our determination is in good agreement with the values in the literature if we assume a low dust-to-gas ratio (similar to 2000 times lower than the Milky Way value). C1 [Lebouteiller, V.] Univ Paris Diderot, Lab AIM, Serv Astrophys, CEA,DSM,CNRS,DAPNIA,CEA Saclay, F-91191 Gif Sur Yvette, France. [Heap, S.] NASA, Lab Astron & Solar Phys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hubeny, I.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Hubeny, I.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kunth, D.] Inst Astrophys, F-75014 Paris, France. RP Lebouteiller, V (reprint author), Univ Paris Diderot, Lab AIM, Serv Astrophys, CEA,DSM,CNRS,DAPNIA,CEA Saclay, Bat 709, F-91191 Gif Sur Yvette, France. EM vianney.lebouteiller@cea.fr OI Lebouteiller, Vianney/0000-0002-7716-6223 FU CEA/Marie Curie Eurotalents fellowship; NASA [NAS5-26555]; NASA Cosmic Origins Spectrograph program at the University of Colorado, Boulder FX V.L. is supported by a CEA/Marie Curie Eurotalents fellowship. We would like to thank Aurelie Remy for the Herschel dust mass measurements. Based on observations obtained with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. S. R. H. and I. H. gratefully acknowledge support by the NASA Cosmic Origins Spectrograph program at the University of Colorado, Boulder. NR 149 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR A16 DI 10.1051/0004-6361/201220948 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700016 ER PT J AU Valori, G Demoulin, P Pariat, E Masson, S AF Valori, G. Demoulin, P. Pariat, E. Masson, S. TI Accuracy of magnetic energy computations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; methods: numerical; Sun: surface magnetism; Sun: corona ID CORONAL MASS EJECTIONS; FORCE-FREE FIELDS; FLUX ROPES; SOLAR-FLARES; EVOLUTION; TRANSITION; HELICITY; ERUPTION AB Context. For magnetically driven events, the magnetic energy of the system is the prime energy reservoir that fuels the dynamical evolution. In the solar context, the free energy (i.e., the energy in excess of the potential field energy) is one of the main indicators used in space weather forecasts to predict the eruptivity of active regions. A trustworthy estimation of the magnetic energy is therefore needed in three-dimensional (3D) models of the solar atmosphere, e. g., in coronal fields reconstructions or numerical simulations. Aims. The expression of the energy of a system as the sum of its potential energy and its free energy (Thomson's theorem) is strictly valid when the magnetic field is exactly solenoidal. For numerical realizations on a discrete grid, this property may be only approximately fulfilled. We show that the imperfect solenoidality induces terms in the energy that can lead to misinterpreting the amount of free energy present in a magnetic configuration. Methods. We consider a decomposition of the energy in solenoidal and nonsolenoidal parts which allows the unambiguous estimation of the nonsolenoidal contribution to the energy. We apply this decomposition to six typical cases broadly used in solar physics. We quantify to what extent the Thomson theorem is not satisfied when approximately solenoidal fields are used. Results. The quantified errors on energy vary from negligible to significant errors, depending on the extent of the nonsolenoidal component of the field. We identify the main source of errors and analyze the implications of adding a variable amount of divergence to various solenoidal fields. Finally, we present pathological unphysical situations where the estimated free energy would appear to be negative, as found in some previous works, and we identify the source of this error to be the presence of a finite divergence. Conclusions. We provide a method of quantifying the effect of a finite divergence in numerical fields, together with detailed diagnostics of its sources. We also compare the efficiency of two divergence-cleaning techniques. These results are applicable to a broad range of numerical realizations of magnetic fields. C1 [Valori, G.; Demoulin, P.; Pariat, E.] Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Valori, G.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Masson, S.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Valori, G (reprint author), Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. EM gherardo.valori@obspm.fr OI Valori, Gherardo/0000-0001-7809-0067 FU European Commission [284461]; NASA FX The authors are pleased to thank Guillaume Aulanier for fruitful discussions, Bernhard Kliem and Tibor Torok for making the numerical solution of the TD equilibrium available, and the referee for helpful comments that improved the clarity of the paper. G.V. is indebted to the NLFFF Consortium for stimulating discussions and collaborations. The research leading to these results has received funding from the European Commission's Seventh Framework Program (FP7/2007-2013) under the grant agreement eHeroes (project no 284461, www.eheroes.eu). S.M. gratefully acknowledges support from the NASA Postdoctoral Program, administrated by Oak Ridge Associated University through a contract with NASA, during her stay at NASA Goddard Space Flight Center. Calculations were done on the quadri-core bi-Xeon computers of the Cluster of the Division Informatique de l'Observatoire de Paris (DIO). SDO data are courtesy of NASA/SDO and the HMI science team. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA (USA), ESA, and NSC (Norway). NR 36 TC 8 Z9 8 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR A38 DI 10.1051/0004-6361/201220982 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700038 ER PT J AU Seager, R Ting, MF Li, CH Naik, N Cook, B Nakamura, J Liu, HB AF Seager, Richard Ting, Mingfang Li, Cuihua Naik, Naomi Cook, Ben Nakamura, Jennifer Liu, Haibo TI Projections of declining surface-water availability for the southwestern United States SO NATURE CLIMATE CHANGE LA English DT Article ID NORTH-AMERICA; HYDROLOGICAL CYCLE; COLORADO RIVER; CLIMATE-CHANGE; PRECIPITATION; RESPONSES; MODEL; US AB Global warming driven by rising greenhouse-gas concentrations is expected to cause wet regions of the tropics and mid to high latitudes to get wetter and subtropical dry regions to get drier and expand polewards(1-4). Over southwest North America, models project a steady drop in precipitation minus evapotranspiration, P - E, the net flux of water at the land surface(5-7), leading to, for example, a decline in Colorado River flow(8-11). This would cause widespread and important social and ecological consequences(12-14). Here, using new simulations from the Coupled Model Intercomparison Project Five, to be assessed in Intergovernmental Panel on Climate Change Assessment Report Five, we extend previous work by examining changes in P, E, runoff and soil moisture by season and for three different water resource regions. Focusing on the near future, 2021-2040, the new simulations project declines in surface-water availability across the southwest that translate into reduced soil moisture and runoff in California and Nevada, the Colorado River headwaters and Texas. C1 [Seager, Richard; Ting, Mingfang; Li, Cuihua; Naik, Naomi; Nakamura, Jennifer; Liu, Haibo] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Cook, Ben] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Seager, R (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. EM seager@ldeo.columbia.edu RI Cook, Benjamin/H-2265-2012 FU NOAA [NA08OAR4320912, NA10OAR4310137]; NSF [AGS-08-04107] FX This work was supported by NOAA awards NA08OAR4320912 and NA10OAR4310137 and NSF award AGS-08-04107. The comments of the wider Global Decadal Hydroclimate Variability and Change (GloDecH) group at Lamont are greatly appreciated. NR 28 TC 75 Z9 75 U1 11 U2 106 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD MAY PY 2013 VL 3 IS 5 BP 482 EP 486 DI 10.1038/NCLIMATE1787 PG 5 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 150PA UT WOS:000319402000014 ER PT J AU Brotton, SJ Kaiser, RI AF Brotton, Stephen J. Kaiser, Ralf I. TI Novel high-temperature and pressure-compatible ultrasonic levitator apparatus coupled to Raman and Fourier transform infrared spectrometers SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID ACOUSTIC LEVITATION; AIRBORNE CHEMISTRY; OPTICAL-PROPERTIES; AMINO-ACIDS; SPECTROSCOPY; SURFACE; SCATTERING; DYNAMICS; SCIENCE; SYSTEMS AB We describe an original apparatus comprising of an acoustic levitator enclosed within a pressure-compatible process chamber. To characterize any chemical and physical modifications of the levitated particle, the chamber is interfaced to complimentary, high-sensitivity Raman (4390-170 cm(-1)), and Fourier transform infrared (FTIR) (10 000-500 cm(-1)) spectroscopic probes. The temperature of the levitated particle can be accurately controlled by heating using a carbon dioxide laser emitting at 10.6 mu m. The advantages of levitating a small particle combined with the two spectroscopic probes, process chamber, and infrared laser heating makes novel experiments possible relevant to the fields of, for example, planetary science, astrobiology, and combustion chemistry. We demonstrate that this apparatus is well suited to study the dehydration of a variety of particles including minerals and biological samples; and offers the possibility of investigating combustion processes involving micrometer-sized particles such as graphite. Furthermore, we show that the FTIR spectrometer enables the study of chemical reactions on the surfaces of porous samples and scientifically and technologically relevant, micrometer-thick levitated sheets. The FTIR spectrometer can also be used to investigate non-resonant and resonant scattering from small, irregularly-shaped particles across the mid-infrared range from 2.5 mu m to 25 mu m, which is relevant to scattering from interplanetary dust and biological, micrometer-sized samples but cannot be accurately modelled using Mie theory. (C) 2013 AIP Publishing LLC. C1 [Brotton, Stephen J.; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Brotton, Stephen J.; Kaiser, Ralf I.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Brotton, SJ (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. FU National Aeronautics and Space Administration (NASA Astrobiology Institute through the Office of Space Science) [NNA09DA77A] FX The material presented in this paper was based upon work supported by the National Aeronautics and Space Administration (NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science). NR 43 TC 6 Z9 6 U1 2 U2 38 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD MAY PY 2013 VL 84 IS 5 AR 055114 DI 10.1063/1.4804647 PG 11 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 158UO UT WOS:000319999300072 PM 23742596 ER PT J AU Chung, SJ Bandyopadhyay, S Chang, I Hadaegh, FY AF Chung, Soon-Jo Bandyopadhyay, Saptarshi Chang, Insu Hadaegh, Fred Y. TI Phase synchronization control of complex networks of Lagrangian systems on adaptive digraphs SO AUTOMATICA LA English DT Article DE Co-operative control; Complex network; Synchronization; Nonlinear control; Adaptive control; Robotics; Space vehicles ID CONTRACTION ANALYSIS; CONCURRENT SYNCHRONIZATION; CONSENSUS ALGORITHMS; MULTIAGENT SYSTEMS; SPACECRAFT; PASSIVITY; COORDINATION; STABILITY; TOPOLOGY; TRACKING AB This paper presents a formation control and synchronization method that utilizes adaptive network topologies for a class of complex dynamical networks comprised of a large number of highly-nonlinear Euler-Lagrange (EL) systems. A time-varying and switching network topology, constructed by the adaptive graph Laplacian matrix, relaxes the standard requirement of consensus stability, even permitting exponential synchronization on an unbalanced digraph or a weakly connected digraph that can sporadically lose connectivity. The time-varying graph Laplacian matrix is adapted by an adaptive control scheme based on relative positions and errors of synchronization and tracking. The adaptive graph Laplacian is integrated with a phase synchronization controller that synchronizes the relative motions of EL systems moving in elliptical orbits, thereby yielding a smaller synchronization error than an uncoupled tracking control law in the presence of bounded disturbances and modeling errors. An example of reconfiguring hundreds of spacecraft in Low Earth Orbit shows the effectiveness of the proposed phase synchronization controller for a large number of complex EL systems moving in periodic elliptical orbits. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Chung, Soon-Jo; Bandyopadhyay, Saptarshi; Chang, Insu] Univ Illinois, Urbana, IL 61801 USA. [Hadaegh, Fred Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chung, SJ (reprint author), Univ Illinois, Urbana, IL 61801 USA. EM sjchung@illinois.edu; bandyop2@illinois.edu; chang162@illinois.edu; fred.y.hadaegh@jpl.nasa.gov OI Chung, Soon-Jo/0000-0002-6657-3907 FU AFOSR [FA95501210193] FX S.-J. Chung and S. Bandyopadhyay were supported in part by the AFOSR grant (FA95501210193). The material in this paper was presented at the 49th IEEE Conference on Decision and Control (CDC), December 15-17, 2010, Atlanta, Georgia, USA, and the AIM Guidance, Navigation, and Control Conference (GNC), August 8-11, 2011, Portland, Oregon, USA. This paper was recommended for publication in revised form by Associate Editor Raul Ordonez under the direction of Editor Miroslav Krstic. NR 48 TC 24 Z9 26 U1 0 U2 48 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0005-1098 J9 AUTOMATICA JI Automatica PD MAY PY 2013 VL 49 IS 5 BP 1148 EP 1161 DI 10.1016/j.automatica.2013.01.048 PG 14 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 146MX UT WOS:000319096300006 ER PT J AU Carson, JM Acikmese, B Murray, RM MacMartin, DG AF Carson, John M., III Acikmese, Behcet Murray, Richard M. MacMartin, Douglas G. TI A robust model predictive control algorithm augmented with a reactive safety mode SO AUTOMATICA LA English DT Article DE Model predictive control; Receding horizon control; Safety mode; Linear matrix inequalities; Robust nonlinear control ID CONSTRAINED LINEAR-SYSTEMS; RECEDING HORIZON CONTROL; STABILITY; TUBES AB A reactive safety mode is built into a robust model predictive control algorithm for uncertain nonlinear systems with bounded disturbances. The algorithm enforces state and control constraints and blends two modes: (I) standard, guarantees re-solvability and asymptotic convergence in a robust receding-horizon manner; (II) safety, if activated, guarantees containment within an invariant set about a reference. The reactive safety mode provides robustness to unexpected, but real-time anticipated, state-constraint changes during standard mode operation. The safety-mode control policy is designed offline and can be activated at any arbitrary time. The standard-mode control has feedforward and feedback components: feedforward is from online solution of a finite-horizon optimal control problem; feedback is designed offline to provide robustness to system uncertainty and disturbances and to establish an invariant "state tube" that guarantees standard-mode re-solvability at any time. The algorithm design is shown for a class of systems with incrementally-conic uncertain/nonlinear terms and bounded disturbances. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Carson, John M., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Acikmese, Behcet] Univ Texas Austin, Austin, TX 78712 USA. [Murray, Richard M.; MacMartin, Douglas G.] CALTECH, Pasadena, CA 91125 USA. RP Carson, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM John.M.Carson@nasa.gov; behcet@austin.utexas.edu; murray@cds.caltech.edu; macmardg@cds.caltech.edu RI MacMartin, Douglas/A-6333-2016; OI MacMartin, Douglas/0000-0003-1987-9417; Murray, Richard/0000-0002-5785-7481 FU AFOSR MURI [FA9550-06-1-0303]; JPL internal RD; Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration FX This research was funded by AFOSR MURI grant FA9550-06-1-0303 and JPL internal R&D. The material in this paper was partially presented at the 17th IFAC World Congress, July 6-11, 2008, Seoul, South Korea. This paper was recommended for publication in revised form by Associate Editor Dragan Nesic under the direction of Editor Andrew R. Teel. (C)2013 California Institute of Technology. Government sponsorship acknowledged.; Publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 28 TC 6 Z9 7 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0005-1098 J9 AUTOMATICA JI Automatica PD MAY PY 2013 VL 49 IS 5 BP 1251 EP 1260 DI 10.1016/j.automatica.2013.02.025 PG 10 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 146MX UT WOS:000319096300016 ER PT J AU Renno, NO Williams, E Rosenfeld, D Fischer, DG Fischer, J Kremic, T Agrawal, A Andreae, MO Bierbaum, R Blakeslee, R Boerner, A Bowles, N Christian, H Cox, A Dunion, J Horvath, A Huang, XL Khain, A Kinne, S Lemos, MC Penner, JE Poschl, U Quaas, J Seran, E Stevens, B Walati, T Wagner, T AF Renno, Nilton O. Williams, Earle Rosenfeld, Daniel Fischer, David G. Fischer, Juergen Kremic, Tibor Agrawal, Arun Andreae, Meinrat O. Bierbaum, Rosina Blakeslee, Richard Boerner, Anko Bowles, Neil Christian, Hugh Cox, Ann Dunion, Jason Horvath, Akos Huang, Xianglei Khain, Alexander Kinne, Stefan Lemos, Maria C. Penner, Joyce E. Poeschl, Ulrich Quaas, Johannes Seran, Elena Stevens, Bjorn Walati, Thomas Wagner, Thomas TI CHASER An Innovative Satellite Mission Concept to Measure the Effects of Aerosols on Clouds and Climate SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID CONVECTIVE CLOUDS; OPTICAL-THICKNESS; DROPLET SIZES; PRECIPITATION; STRATOCUMULUS; MICROPHYSICS; ENTRAINMENT; ATMOSPHERE; REGIMES; NUMBER AB The formation of cloud droplets on aerosol particles, technically known as the activation of cloud condensation nuclei (CCN), is the fundamental process driving the interactions of aerosols with clouds and precipitation. The Intergovernmental Panel on Climate Change (IPCC) and the Decadal Survey indicate that the uncertainty in how clouds adjust to aerosol perturbations dominates the uncertainty in the overall quantification of the radiative forcing attributable to human activities. Measurements by current satellites allow the determination of crude profiles of cloud particle size, but not of the activated CCN that seed them. The Clouds, Hazards, and Aerosols Survey for Earth Researchers (CHASER) mission concept responds to the IPCC and Decadal Survey concerns, utilizing a new technique and high-heritage instruments to measure all the quantities necessary to produce the first global survey maps of activated CCN and the properties of the clouds associated with them. CHASER also determines the activated CCN concentration and cloud thermodynamic forcing simultaneously, allowing the effects of each to be distinguished. C1 [Renno, Nilton O.; Huang, Xianglei; Penner, Joyce E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Williams, Earle] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. [Rosenfeld, Daniel; Khain, Alexander] Hebrew Univ Jerusalem, Jerusalem, Israel. [Fischer, David G.; Kremic, Tibor] NASA, Glenn Res Ctr, Cleveland, OH USA. [Fischer, Juergen] Free Univ Berlin, Berlin, Germany. [Agrawal, Arun; Bierbaum, Rosina; Lemos, Maria C.] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. [Andreae, Meinrat O.; Poeschl, Ulrich] Max Planck Inst Chem, D-55128 Mainz, Germany. [Blakeslee, Richard] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Boerner, Anko; Walati, Thomas] Deutsch Zentrum Luft & Raumfahrt DLR, Berlin, Germany. [Bowles, Neil] Univ Oxford, Oxford, England. [Christian, Hugh] Univ Alabama, ESSC NSSTC, Huntsville, AL 35899 USA. [Cox, Ann] Orbital Sci Corp, Dulles, VA USA. [Dunion, Jason] Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL USA. [Horvath, Akos; Kinne, Stefan; Stevens, Bjorn] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Quaas, Johannes] Univ Leipzig, Inst Meteorol, D-04109 Leipzig, Germany. [Seran, Elena] Univ Paris 06, LATMOS, Paris, France. [Wagner, Thomas] Heidelberg Univ, Inst Umweltphys, Heidelberg, Germany. RP Renno, NO (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA. EM renno@alum.mit.edu RI Huang, Xianglei/G-6127-2011; Horvath, Akos/A-2453-2008; Penner, Joyce/J-1719-2012; Stevens, Bjorn/A-1757-2013; Poschl, Ulrich/A-6263-2010; Dunion, Jason/B-1352-2014; Rosenfeld, Daniel/F-6077-2016; Quaas, Johannes/I-2656-2013; Andreae, Meinrat/B-1068-2008 OI Huang, Xianglei/0000-0002-7129-614X; Horvath, Akos/0000-0002-5860-2368; Stevens, Bjorn/0000-0003-3795-0475; Poschl, Ulrich/0000-0003-1412-3557; Dunion, Jason/0000-0001-7489-0569; Rosenfeld, Daniel/0000-0002-0784-7656; Quaas, Johannes/0000-0001-7057-194X; Andreae, Meinrat/0000-0003-1968-7925 FU NSF [AGS 1118467] FX We thank NASA Glenn Research Center, the University of Michigan, the Deutsches Zentrum fur Luft- und Raumfahrt (DLR), the Israeli Space Agency, and Orbital Sciences Corporation for supporting the development of the CHASER mission concept. Many engineers, managers, and technical staff played key roles on the development of the CHASER mission concept. N. Renno was partially supported by NSF Award AGS 1118467. NR 49 TC 7 Z9 7 U1 2 U2 23 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 MAY PY 2013 VL 94 IS 5 BP 685 EP + DI 10.1175/BAMS-D-11-00239.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 150DT UT WOS:000319371100017 ER PT J AU Long, CN McFarlane, SA Del Genio, A Minnis, P Ackerman, TP Mather, J Comstock, J Mace, GG Jensen, M Jakob, C AF Long, C. N. McFarlane, S. A. Del Genio, A. Minnis, P. Ackerman, T. P. Mather, J. Comstock, J. Mace, G. G. Jensen, M. Jakob, C. TI ARM RESEARCH IN THE EQUATORIAL WESTERN PACIFIC A DECADE AND COUNTING SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID RADIATION MEASUREMENT PROGRAM; MADDEN-JULIAN OSCILLATION; CLIMATE RESEARCH FACILITY; MILLIMETER RADAR DATA; COLUMN WATER-VAPOR; CLOUD-TOP HEIGHT; ATMOSPHERIC RADIATION; TROPICAL CIRRUS; NAURU-ISLAND; SATELLITE-OBSERVATIONS AB The tropical western Pacific (TWP) is an important climatic region. Strong solar heating, warm sea surface temperatures, and the annual progression of the intertropical convergence zone (ITCZ) across this region generate abundant convective systems, which through their effects on the heat and water budgets have a profound impact on global climate and precipitation. In order to accurately evaluate tropical cloud systems in models, measurements of tropical clouds, the environment in which they reside, and their impact on the radiation and water budgets are needed. Because of the remote location, ground-based datasets of cloud, atmosphere, and radiation properties from the TWP region have come primarily from short-term field experiments. While providing extremely useful information on physical processes, these short-term datasets are limited in statistical and climatological information. To provide long-term measurements of the surface radiation budget in the tropics and the atmospheric properties that affect it, the Atmospheric Radiation Measurement program established a measurement site on Manus Island, Papua New Guinea, in 1996 and on the island republic of Nauru in late 1998. These sites provide unique datasets now available for more than 10 years on Manus and Nauru. This article presents examples of the scientific use of these datasets including characterization of cloud properties, analysis of cloud radiative forcing, model studies of tropical clouds and processes, and validation of satellite algorithms. New instrumentation recently installed at the Manus site will provide expanded opportunities for tropical atmospheric science. C1 [Long, C. N.; McFarlane, S. A.; Mather, J.; Comstock, J.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Del Genio, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Minnis, P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Ackerman, T. P.] Univ Washington, JISAO, Seattle, WA 98195 USA. [Mace, G. G.] Univ Utah, Salt Lake City, UT USA. [Jensen, M.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Jakob, C.] Monash Univ, Melbourne, Vic 3004, Australia. RP Long, CN (reprint author), Pacific NW Natl Lab, POB 999,MSIN K4-28, Richland, WA 99352 USA. EM chuck.long@pnl.gov RI Jakob, Christian/A-1082-2010; Minnis, Patrick/G-1902-2010 OI Jakob, Christian/0000-0002-5012-3207; Minnis, Patrick/0000-0002-4733-6148 NR 71 TC 14 Z9 14 U1 0 U2 14 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 MAY PY 2013 VL 94 IS 5 BP 695 EP + DI 10.1175/BAMS-D-11-00137.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 150DT UT WOS:000319371100018 ER PT J AU Ballance, CP Loch, SD Foster, AR Smith, RK Witthoeft, MC Kallman, TR AF Ballance, C. P. Loch, S. D. Foster, A. R. Smith, R. K. Witthoeft, M. C. Kallman, T. R. TI UNCERTAINTIES ON ATOMIC DATA SO FUSION SCIENCE AND TECHNOLOGY LA English DT Article; Proceedings Paper CT Technical Meeting on Data Evaluation for Atomic, Molecular and Plasma-Material Interaction Processes in Fusion CY SEP 04-07, 2012 CL Daejeon, SOUTH KOREA DE uncertainty estimates on atomic data; collisional radiative modeling; R-matrix ID ELECTRON-IMPACT EXCITATION; RECOMBINATION; PLASMAS; IONS AB There have been long outstanding requests from the modeling community for uncertainty estimates on atomic data. This paper outlines a systematic approach from fundamental atomic structure and collisional calculations, through to well-known spectral diagnostic lines, correlating the uncertainties from each contributing process. C1 [Ballance, C. P.; Loch, S. D.] Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA. [Foster, A. R.; Smith, R. K.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Witthoeft, M. C.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ballance, CP (reprint author), Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA. EM ballance@physics.auburn.edu FU U.S. Department of Energy FX C. P. B. acknowledges the invitation by the International Atomic Energy Agency (IAEA) and the support of the National Fusion Research Institute (NFRI) for his participation in the Joint IAEA-NFRI Technical Meeting on Data Evaluation. A part of this work was funded by the U.S. Department of Energy, and the O VII calculations were carried out at the National Energy Research Scientific Computing Center computing facilities in Berkeley, California. NR 7 TC 1 Z9 1 U1 0 U2 8 PU AMER NUCLEAR SOC PI LA GRANGE PK PA 555 N KENSINGTON AVE, LA GRANGE PK, IL 60526 USA SN 1536-1055 EI 1943-7641 J9 FUSION SCI TECHNOL JI Fusion Sci. Technol. PD MAY PY 2013 VL 63 IS 3 BP 358 EP 362 PG 5 WC Nuclear Science & Technology SC Nuclear Science & Technology GA 148KX UT WOS:000319244600007 ER PT J AU Noh, Y Lee, U Wang, P Choi, BSC Gerla, M AF Noh, Youngtae Lee, Uichin Wang, Paul Choi, Brian Sung Chul Gerla, Mario TI VAPR: Void-Aware Pressure Routing for Underwater Sensor Networks SO IEEE TRANSACTIONS ON MOBILE COMPUTING LA English DT Article DE Pressure routing; anycast; opportunistic routing ID AD HOC; WIRELESS NETWORKS; PROTOCOL AB Underwater mobile sensor networks have recently been proposed as a way to explore and observe the ocean, providing 4D (space and time) monitoring of underwater environments. We consider a specialized geographic routing problem called pressure routing that directs a packet to any sonobuoy on the surface based on depth information available from on-board pressure gauges. The main challenge of pressure routing in sparse underwater networks has been the efficient handling of 3D voids. In this respect, it was recently proven that the greedy stateless perimeter routing method, very popular in 2D networks, cannot be extended to void recovery in 3D networks. Available heuristics for 3D void recovery require expensive flooding. In this paper, we propose a Void-Aware Pressure Routing (VAPR) protocol that uses sequence number, hop count and depth information embedded in periodic beacons to set up next-hop direction and to build a directional trail to the closest sonobuoy. Using this trail, opportunistic directional forwarding can be efficiently performed even in the presence of voids. The contribution of this paper is twofold: 1) a robust soft-state routing protocol that supports opportunistic directional forwarding; and 2) a new framework to attain loop freedom in static and mobile underwater networks to guarantee packet delivery. Extensive simulation results show that VAPR outperforms existing solutions. C1 [Noh, Youngtae; Gerla, Mario] Univ Calif Los Angeles, Dept Comp Sci, Los Angeles, CA 90095 USA. [Lee, Uichin] Korea Adv Inst Sci & Technol, Dept Knowledge Serv Engn, Taejon 305701, South Korea. [Wang, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Choi, Brian Sung Chul] Google Inc, Mountain View, CA 94043 USA. RP Noh, Y (reprint author), Univ Calif Los Angeles, Dept Comp Sci, 3803B Boelter Hall, Los Angeles, CA 90095 USA. EM ytnoh@cs.ucla.edu; uclee@kaist.edu; Paul.Wang@jpl.nasa.gov; sungchoi@google.com; gerla@cs.ucla.edu RI Lee, Uichin/C-1827-2011 NR 53 TC 35 Z9 39 U1 1 U2 21 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1536-1233 EI 1558-0660 J9 IEEE T MOBILE COMPUT JI IEEE. Trans. Mob. Comput. PD MAY PY 2013 VL 12 IS 5 BP 895 EP 908 DI 10.1109/TMC.2012.53 PG 14 WC Computer Science, Information Systems; Telecommunications SC Computer Science; Telecommunications GA 150QZ UT WOS:000319407200007 ER PT J AU Ray, RD Luthcke, SB van Dam, T AF Ray, R. D. Luthcke, S. B. van Dam, T. TI Monthly Crustal Loading Corrections for Satellite Altimetry SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID MEAN SEA-LEVEL; HEIGHT TIME-SERIES; GEOCENTER MOTION; MASS VARIATION; SOLID EARTH; GRACE; GPS; DEFORMATION; VARIABILITY; MODELS AB Satellite altimeter measurements of sea surface height include a small contribution from vertical motion of the seafloor caused by crustal loading. Loading by ocean tides is routinely allowed for in altimeter data processing. Here, loading by nontidal fluids of the atmosphere, ocean, and terrestrial hydrosphere is examined. The crustal deformation can be computed from either geophysical models or from Gravity Recovery and Climate Experiment (GRACE) gravity inversions of mass variability. The loading corrections are found to be very small, rarely exceeding a few millimeters. Nonetheless, they form a significant correction to altimetric determinations of global mean sea level. The correction is most important at the annual cycle and should be accounted for when attempting to balance the global sea level budget. C1 [Ray, R. D.; Luthcke, S. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [van Dam, T.] Univ Luxembourg, Walferdange, Luxembourg. RP Ray, RD (reprint author), NASA GSFC, Code 698, Greenbelt, MD 20771 USA. EM richard.ray@nasa.gov RI Ray, Richard/D-1034-2012 FU NASA IDS Sea Level investigation; NASA GRACE investigation FX This work was supported by NASA IDS Sea Level and GRACE investigations. Jean-Paul Boy provided essential help in obtaining the geophysical fluid models. We thank Frank Lemoine, David Rowlands, and John Ries for the useful discussions. NR 40 TC 0 Z9 0 U1 1 U2 11 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 MAY PY 2013 VL 30 IS 5 BP 999 EP 1005 DI 10.1175/JTECH-D-12-00152.1 PG 7 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 148PW UT WOS:000319259000010 ER PT J AU Fenty, I Heimbach, P AF Fenty, Ian Heimbach, Patrick TI Hydrographic Preconditioning for Seasonal Sea Ice Anomalies in the Labrador Sea SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID NORTH-ATLANTIC CIRCULATION; DEEP CONVECTION; GREENLAND SEA; UPPER OCEAN; BOUNDARY-LAYER; BAFFIN-BAY; MODEL; FLUCTUATIONS; ADJOINT; COVER AB This study investigates the hydrographic processes involved in setting the maximum wintertime sea ice (SI) extent in the Labrador Sea and Baffin Bay. The analysis is based on an ocean and sea ice state estimate covering the summer-to-summer 1996/97 annual cycle. The estimate is a synthesis of in situ and satellite hydrographic and ice data with a regional coupled 1/3 degrees ocean-sea ice model. SI advective processes are first demonstrated to be required to reproduce the observed ice extent. With advection, the marginal ice zone (MIZ) location stabilizes where ice melt balances ice mass convergence, a quasi-equilibrium condition achieved via the convergence of warm subtropical-origin subsurface waters into the mixed layer seaward of the MIZ. An analysis of ocean surface buoyancy fluxes reveals a critical role of low-salinity upper ocean (100 m) anomalies for the advancement of SI seaward of the Arctic Water-Irminger Water Thermohaline Front. Anomalous low-salinity waters slow the rate of buoyancy loss-driven mixed layer deepening, shielding an advancing SI pack from the warm subsurface waters, and are conducive to a positive surface meltwater stabilization enhancement (MESEM) feedback driven by SI meltwater release. The low-salinity upper-ocean hydrographic conditions in which the MESEM efficiently operates are termed sea ice-preconditioned waters (SIPW). The SI extent seaward of the Thermohaline Front is shown to closely correspond to the distribution of SIPW. The analysis of two additional state estimates (1992/93, 2003/04) suggests that interannual hydrographic variability provides a first-order explanation for SI maximum extent anomalies in the region. C1 [Fenty, Ian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Heimbach, Patrick] MIT, Cambridge, MA 02139 USA. RP Fenty, I (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ian.fenty@jpl.nasa.gov RI Heimbach, Patrick/K-3530-2013 OI Heimbach, Patrick/0000-0003-3925-6161 FU NASA [NNX11AQ12G]; NSF [ARC-1023499] FX The authors would like to acknowledge Carl Wunsch for providing valuable guidance during the course of this research and the preparation of the final manuscript. This research was carried out in part by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA and in part through NSF Grant ARC-1023499, NASA's MAP Grant NNX11AQ12G, and the ECCO-GODAE project. We thank our ECCO-GODAE partners, the MITgcm development group, and the various data centers for making their data available. NR 54 TC 3 Z9 3 U1 1 U2 15 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD MAY PY 2013 VL 43 IS 5 BP 863 EP 883 DI 10.1175/JPO-D-12-064.1 PG 21 WC Oceanography SC Oceanography GA 154IV UT WOS:000319669100003 ER PT J AU Fenty, I Heimbach, P AF Fenty, Ian Heimbach, Patrick TI Coupled Sea Ice-Ocean-State Estimation in the Labrador Sea and Baffin Bay SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID WESTERN BOUNDARY CURRENTS; NORTH-ATLANTIC SST; FRESH-WATER; GREENLAND SEA; HEAT FLUXES; WINTER CIRCULATION; DEEP CONVECTION; MODEL; EDDIES; COVER AB Sea ice variability in the Labrador Sea is of climatic interest because of its relationship to deep convection, mode-water formation, and the North Atlantic atmospheric circulation. Historically, quantifying the relationship between sea ice and ocean variability has been difficult because of in situ observation paucity and technical challenges associated with synthesizing observations with numerical models. Here the relationship between ice and ocean variability is explored by analyzing new estimates of the ocean-ice state in the northwest North Atlantic. The estimates are syntheses of in situ and satellite hydrographic and ice data with a regional 1/3 degrees coupled ocean-sea ice model. The synthesis of sea ice data is achieved with an improved adjoint of a thermodynamic ice model. Model and data are made consistent, in a least squares sense, by iteratively adjusting control variables, including ocean initial and lateral boundary conditions and the atmospheric state, to minimize an uncertainty-weighted model-data misfit cost function. The utility of the state estimate is demonstrated in an analysis of energy and buoyancy budgets in the marginal ice zone (MIZ). In mid-March the system achieves a state of quasi-equilibrium during which net ice growth and melt approaches zero; newly formed ice diverges from coastal areas and converges via wind and ocean forcing in the MIZ. The convergence of ice mass in the MIZ is ablated primarily by turbulent ocean-ice enthalpy fluxes. The primary source of the enthalpy required for sustained MIZ ice ablation is the sensible heat reservoir of the subtropical-origin subsurface waters. C1 [Fenty, Ian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Heimbach, Patrick] MIT, Cambridge, MA 02139 USA. RP Fenty, I (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ian.fenty@jpl.nasa.gov RI Heimbach, Patrick/K-3530-2013 OI Heimbach, Patrick/0000-0003-3925-6161 FU NASA [NNX11AQ12G]; NSF [ARC-1023499] FX The authors would like to acknowledge Carl Wunsch for providing valuable guidance during the course of this research and the preparation of the final manuscript. This research was carried out in part by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA and in part through NSF Grant ARC-1023499, NASA's MAP Grant NNX11AQ12G, and the ECCO-GODAE project. We thank our ECCO-GODAE partners, the MITgcm development group, and the various data centers for making their data available. NR 90 TC 11 Z9 11 U1 3 U2 22 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD MAY PY 2013 VL 43 IS 5 BP 884 EP 904 DI 10.1175/JPO-D-12-065.1 PG 21 WC Oceanography SC Oceanography GA 154IV UT WOS:000319669100004 ER PT J AU Forkel, M Carvalhais, N Verbesselt, J Mahecha, MD Neigh, CSR Reichstein, M AF Forkel, Matthias Carvalhais, Nuno Verbesselt, Jan Mahecha, Miguel D. Neigh, Christopher S. R. Reichstein, Markus TI Trend Change Detection in NDVI Time Series: Effects of Inter-Annual Variability and Methodology SO REMOTE SENSING LA English DT Article DE greening; browning; breakpoints; seasonal cycle; season-trend model; boreal; forest tundra; fire; disturbances; Alaska ID SPECTRAL VEGETATION INDEXES; SATELLITE DATA; NORTH-AMERICA; BOREAL FOREST; EL-NINO; ALASKA; MODIS; CLIMATE; DISTURBANCE; ACCURACY AB Changing trends in ecosystem productivity can be quantified using satellite observations of Normalized Difference Vegetation Index (NDVI). However, the estimation of trends from NDVI time series differs substantially depending on analyzed satellite dataset, the corresponding spatiotemporal resolution, and the applied statistical method. Here we compare the performance of a wide range of trend estimation methods and demonstrate that performance decreases with increasing inter-annual variability in the NDVI time series. Trend slope estimates based on annual aggregated time series or based on a seasonal-trend model show better performances than methods that remove the seasonal cycle of the time series. A breakpoint detection analysis reveals that an overestimation of breakpoints in NDVI trends can result in wrong or even opposite trend estimates. Based on our results, we give practical recommendations for the application of trend methods on long-term NDVI time series. Particularly, we apply and compare different methods on NDVI time series in Alaska, where both greening and browning trends have been previously observed. Here, the multi-method uncertainty of NDVI trends is quantified through the application of the different trend estimation methods. Our results indicate that greening NDVI trends in Alaska are more spatially and temporally prevalent than browning trends. We also show that detected breakpoints in NDVI trends tend to coincide with large fires. Overall, our analyses demonstrate that seasonal trend methods need to be improved against inter-annual variability to quantify changing trends in ecosystem productivity with higher accuracy. C1 [Forkel, Matthias; Carvalhais, Nuno; Mahecha, Miguel D.; Reichstein, Markus] Max Planck Inst Biogeochem, Dept Biogeochem Integrat, D-07745 Jena, Germany. [Carvalhais, Nuno] Univ Nova Lisboa, FCT, P-2829516 Caparica, Portugal. [Verbesselt, Jan] Wageningen Univ, Lab Geoinformat Sci & Remote Sensing, NL-6708 PB Wageningen, Netherlands. [Neigh, Christopher S. R.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Forkel, M (reprint author), Max Planck Inst Biogeochem, Dept Biogeochem Integrat, Hans Knoll Str 10, D-07745 Jena, Germany. EM mforkel@bgc-jena.mpg.de; ncarval@bgc-jena.mpg.de; jan.verbesselt@wur.nl; mmahecha@bgc-jena.mpg.de; christopher.s.neigh@nasa.gov; mreichstein@bgc-jena.mpg.de RI Neigh, Christopher/D-4700-2012; Verbesselt, Jan/B-8029-2015; Mahecha, Miguel/F-2443-2010; OI Neigh, Christopher/0000-0002-5322-6340; Verbesselt, Jan/0000-0001-7923-4309; Mahecha, Miguel/0000-0003-3031-613X; Forkel, Matthias/0000-0003-0363-9697; Carvalhais, Nuno/0000-0003-0465-1436 FU Max Planck Institute for Biogeochemistry and from the European Commission's 7th Framework Programme project CARBONES [242316]; European Commission's 7th Framework Program project Carbo-Extreme [226701]; Marie-Curie IRG grant of the European Commission's 7th Framework Program [268423]; European Commission's 7th Framework Program project GEOCARBON [283080]; NASA's Terrestrial Ecology and Carbon Cycle Science Programs [NNH07ZDA001N-CARBON] FX M.F. received funding from the Max Planck Institute for Biogeochemistry and from the European Commission's 7th Framework Programme project CARBONES (grant agreement 242316). N.C. was supported by the European Commission's 7th Framework Program project Carbo-Extreme (grantagreement 226701). J.V. was supported by a Marie-Curie IRG grant of the European Commission's 7th Framework Program (grant agreement 268423). M.M. was supported by the European Commission's 7th Framework Program project GEOCARBON (grant agreement 283080). C.N. was supported by NASA's Terrestrial Ecology and Carbon Cycle Science Programs (grant agreement NNH07ZDA001N-CARBON). M.F conducted this work under the International Max Planck Research School for Global Biogeochemical Cycles. NR 57 TC 69 Z9 70 U1 8 U2 94 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD MAY PY 2013 VL 5 IS 5 BP 2113 EP 2144 DI 10.3390/rs5052113 PG 32 WC Remote Sensing SC Remote Sensing GA 151CT UT WOS:000319438900005 ER PT J AU Cook, BI Pau, S AF Cook, Benjamin I. Pau, Stephanie TI A Global Assessment of Long-Term Greening and Browning Trends in Pasture Lands Using the GIMMS LAI3g Dataset SO REMOTE SENSING LA English DT Article DE pasture; vegetation productivity; land degradation ID NET PRIMARY PRODUCTIVITY; SHRUB ENCROACHMENT; TIME-SERIES; DATA SETS; SATELLITE-OBSERVATIONS; PHOTOSYNTHETIC TRENDS; CO2 FERTILIZATION; FIRE DISTURBANCE; MESIC GRASSLAND; INNER-MONGOLIA AB Pasture ecosystems may be particularly vulnerable to land degradation due to the high risk of human disturbance (e.g., overgrazing, burning, etc.), especially when compared with natural ecosystems (non-pasture, non-cultivated) where direct human impacts are minimal. Using maximum annual leaf area index (LAImax) as a proxy for standing biomass and peak annual aboveground productivity, we analyze greening and browning trends in pasture areas from 1982-2008. Inter-annual variability in pasture productivity is strongly controlled by precipitation (positive correlation) and, to a lesser extent, temperature (negative correlation). Linear temporal trends are significant in 23% of pasture cells, with the vast majority of these areas showing positive LAImax trends. Spatially extensive productivity declines are only found in a few regions, most notably central Asia, southwest North America, and southeast Australia. Statistically removing the influence of precipitation reduces LAImax trends by only 13%, suggesting that precipitation trends are only a minor contributor to long-term greening and browning of pasture lands. No significant global relationship was found between LAImax and pasture intensity, although the magnitude of trends did vary between cells classified as natural versus pasture. In the tropics and Southern Hemisphere, the median rate of greening in pasture cells is significantly higher than for cells dominated by natural vegetation. In the Northern Hemisphere extra-tropics, conversely, greening of natural areas is 2-4 times the magnitude of greening in pasture areas. This analysis presents one of the first global assessments of greening and browning trends in global pasture lands, including a comparison with vegetation trends in regions dominated bynatural ecosystems. Our results suggest that degradation of pasture lands is not a globally widespread phenomenon and, consistent with much of the terrestrial biosphere, there have been widespread increases in pasture productivity over the last 30 years. C1 [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Cook, Benjamin I.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Pau, Stephanie] Florida State Univ, Dept Geog, Tallahassee, FL 32306 USA. RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM benjamin.i.cook@nasa.gov; spau@fsu.edu FU NASA FX The LAI3g data were graciously provided by Ranga Myneni and Zhaichun Zhu. Support for BI Cook came from NASA. The authors thank four anonymous reviewers whose comments greatly improved the quality of this manuscript. LDEO contribution #7691. NR 88 TC 9 Z9 9 U1 2 U2 34 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD MAY PY 2013 VL 5 IS 5 BP 2492 EP 2512 DI 10.3390/rs5052492 PG 21 WC Remote Sensing SC Remote Sensing GA 151CT UT WOS:000319438900024 ER PT J AU Berejikian, BA Campbell, LA Moore, ME AF Berejikian, Barry A. Campbell, Lance A. Moore, Megan E. TI Large-scale freshwater habitat features influence the degree of anadromy in eight Hood Canal Oncorhynchus mykiss populations SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID RESIDENT RAINBOW-TROUT; SALMON SALMO-SALAR; LIFE-HISTORY; ATLANTIC SALMON; STEELHEAD TROUT; OTOLITH MICROCHEMISTRY; SOCKEYE-SALMON; MATING SYSTEM; YAKIMA RIVER; SEX-RATIO AB Juvenile Oncorhynchus mykiss maternity was determined from otolith strontium: calcium ratios to investigate the degree of anadromy in eight freshwater streams draining to a common fjord. The percentages of O. mykiss parr produced by anadromous females ranged from an annual average of 41.3% (Hamma Hamma River) to 100% (Dewatto River). The proportion of stream habitat available to resident O. mykiss upstream of barriers to anadromous migration explained a significant portion of the variability in maternal life history below barrier falls and was included in each of the five logistic regression models with the lowest AIC scores. Transitional hydrologic profiles, low mean annual temperatures and high mean annual stream flow, common to Olympic Peninsula streams, were each associated with greater proportions of offspring from resident females. Only 2 out of 234 parr from the lowland, rain-driven, low-flow streams of the Kitsap Peninsula were produced by resident females. Thus, large-scale habitat features, and primarily the presence or absence of resident populations above natural barriers to anadromous migration, appeared to shape the degree of anadromy among populations. C1 [Berejikian, Barry A.; Moore, Megan E.] NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester, WA 98353 USA. [Campbell, Lance A.] Washington Dept Fish & Wildlife, Olympia, WA 98501 USA. RP Berejikian, BA (reprint author), NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, POB 130 Manchester, Manchester, WA 98353 USA. EM barry.berejikian@noaa.gov NR 57 TC 10 Z9 10 U1 1 U2 27 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD MAY PY 2013 VL 70 IS 5 BP 756 EP 765 DI 10.1139/cjfas-2012-0491 PG 10 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 148PM UT WOS:000319257700010 ER PT J AU Abbott, EA Gillespie, AR Kahle, AB AF Abbott, Elsa A. Gillespie, Alan R. Kahle, Anne B. TI Thermal-infrared imaging of weathering and alteration changes on the surfaces of basalt flows, Hawai"i, USA SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID EMISSIVITY SEPARATION ALGORITHM; KILAUEA VOLCANO; ROCK COATINGS; LAVA FLOWS; IMAGES; FIELD; TEMPERATURE AB Basaltic pahoehoe lavas weather on time scales of decades to millennia and are chemically altered by volcanic heat and gases on time scales of days to decades following their eruption. Despite differences in reactions and rates, the end products, viewed spectrally in the thermal infrared (TIR: 812 m), are similar and distinctive: initial rinds of quickly cooled, disordered glass with broad emissivity minima at 911 m devitrify to yield a sharper emissivity band at 9.1 m; opaline rinds with a similar emissivity feature accrete and gradually transition to cryptocrystalline quartz with an emissivity minimum near 8.1 m. Ultimately, exposed surfaces are oxidized and hydrated to palagonite, with a loss of spectral contrast and character. We have collected over 600 pahoehoe samples of different ages from seven sites on Mauna Loa and the south coast of Hawaii in order to measure hemispheric emissivity spectra and compare them to airborne and spaceborne TIR Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) AST05 emissivity images of Hawaii. ASTER, with five 90 m TIR bands, has operated over the 11 year period since launch in late 1999. Images and samples from some of the Hawaiian sites were collected repeatedly over a decade or more to study the rate of spectral change there. Continuing eruptions of Puu Oo since 1983 offered an opportunity to study the effects of a persistent dousing of lavas by acidic rain and air (vog'), and older flows from Mauna Loa offered an opportunity to study the effects of weathering away from active vents. Weathering changes and rates quantified spectrally are helpful in mapping and assessing long-term environments on volcanoes. C1 [Abbott, Elsa A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Gillespie, Alan R.; Kahle, Anne B.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. RP Abbott, EA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM arg3@uw.edu FU [NAS 7-03001] FX We thank the following people from the USGS Hawai'ian Volcano Observatory: C. Heliker, J. Kauahikaua, J. Lockwood, T. Moulds, and A. Okamura. D. Sabol, G. Yamada, L. Maldonado, and H. Tan were most helpful in the field. C. Grove ran many spectra for us in the lab. We acknowledge Hawai'i Volcano National Park for issuing collecting permits. We are grateful for a critical reading by Matthew Smith and two anonymous formal reviews that all improved the manuscript. This work was done under contract to NASA (contract no. NAS 7-03001) and with the tacit approval of Mme Pele. NR 24 TC 1 Z9 1 U1 0 U2 14 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD MAY 1 PY 2013 VL 34 IS 9-10 SI SI BP 3332 EP 3355 DI 10.1080/01431161.2012.716920 PG 24 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 147NI UT WOS:000319173900010 ER PT J AU Amici, S Piscini, A Buongiorno, MF Pieri, D AF Amici, S. Piscini, A. Buongiorno, M. F. Pieri, D. TI Geological classification of Volcano Teide by hyperspectral and multispectral satellite data SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID SPACEBORNE THERMAL EMISSION; REFLECTION RADIOMETER ASTER; TENERIFE CANARY-ISLANDS; DATA PRODUCTS; SPECTROSCOPY; STRATIGRAPHY; INSTRUMENT AB Tenerife is the central island of the Canary Archipelago (Spain), which consists of seven islands that represent different stages of geological evolution. The Teide-Pico Viejo (28 degrees 16 30 N, 16 degrees 38 42 W) stratocones formed during the last eruptive phase of the isle of Tenerife. It is an active, though currently quiescent, shield volcano that last erupted in 1909 and is located on the Tenerife Island. In the framework of the European Project FP6 Prevention, Information and Early Warning (PREVIEW)-EURORISK (), a field campaign was performed on Tenerife Island on September 2007. This campaign focused on the acquisition of in situ reflectance and emissivity spectra relative to Pico de Teide and Las Canadas Caldera. The collected spectra represented the ground truth' and have been used for the supervised classification on multispectral (Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER)) and hyperspectral (Earth Observing 1 (EO1)-Hyperion) data. The first ever classification mapping carried out on the Teide Volcano by utilizing the remote-sensing method is reported in this article. The methods used to process and to classify the data are discussed, and a comparison with the existing geological maps is presented. C1 [Amici, S.; Piscini, A.; Buongiorno, M. F.] Ist Nazl Geofis & Vulcanol, Rome, Italy. [Pieri, D.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Amici, S (reprint author), Ist Nazl Geofis & Vulcanol, Rome, Italy. EM stefania.amici@ingv.it FU European Community; NASA Earth Surface and Interior Program at the Jet Propulsion Laboratory of the California Institute of Technology FX We acknowledge the efforts of the INGV-Teide campaign field team, including M. Musacchio, V. Lombardo, S. Corradini, and M.I. Pannaccione Apa. We also acknowledge the kind assistance of the Director of 'Planificacion y Operaciones de Emergencias', Dr Fernando Clavijo Redondo, and Dr Sergio Barrera Rodriguez, Direccion General de Seguridad y Emergencias, Gobierno de Canarias, both of whom made possible our fieldwork campaign throughout the Teide Volcano Natural Park on Tenerife Island. We thank the European Community, which provided funds for the PREVIEW project, and also the NASA ASTER and Hyperion spacecraft teams for their data acquisitions and processing. This work was carried out, in part, under contract to the NASA Earth Surface and Interior Program at the Jet Propulsion Laboratory of the California Institute of Technology. NR 34 TC 3 Z9 3 U1 2 U2 22 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD MAY 1 PY 2013 VL 34 IS 9-10 SI SI BP 3356 EP 3375 DI 10.1080/01431161.2012.716913 PG 20 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 147NI UT WOS:000319173900011 ER PT J AU Dick, SJ AF Dick, Steven J. TI The Stardust Revolution: The New Story of Our Origin in the Stars SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Dick, Steven J.] NASA, Washington, DC USA. [Dick, Steven J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. EM stevedick1@comcast.net NR 1 TC 0 Z9 0 U1 0 U2 1 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD MAY PY 2013 VL 44 BP 219 EP 220 PN 2 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 145PH UT WOS:000319028600011 ER PT J AU Schwerdt, HN Miranda, FA Chae, J AF Schwerdt, Helen N. Miranda, Felix A. Chae, Junseok TI Analysis of Electromagnetic Fields Induced in Operation of a Wireless Fully Passive Backscattering Neurorecording Microsystem in Emulated Human Head Tissue SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article DE Backscattering; brain-machine interfaces; implantable electronics; microelectromechanical systems (MEMS); passive devices; specific absorption rate (SAR) ID EQUIVALENT PHANTOM; DEVICES; SYSTEM; BRAIN AB This paper reports on a fully passive microsystem that wirelessly records and transmits neuropotentials exclusively by means of electromagnetic backscattering techniques, affording substantially simpler circuitry and potentially safer and more reliable approach for implantable wireless neurorecording. A fundamental practical barrier for wireless brain-implantable microsystems includes heat dissipation by on-chip circuitry, which may cause permanent brain damage. Hence, measurement of thermal profiles of surrounding tissue induced by operation of wireless implants is imperative in assessing the safety of these devices. Evaluation of specific absorption rate (SAR) is especially relevant for wireless electromagnetic transmission schemes operating at microwave frequencies and directly relates to the heat generated within biological tissue media. In this study, computational and empirical methods are used to measure SAR within a human-head-equivalent phantom during operation of the embedded fully passive wireless neurorecording microsystem. The maximum average SAR, coinciding with the worst case scenario, measured within 1 g of brain tissue is < 0.45 +/- 0.11 W/kg, complying with the U.S. FCC threshold (1.6 W/kg). C1 [Schwerdt, Helen N.; Chae, Junseok] Arizona State Univ, Dept Elect Engn, Tempe, AZ 85287 USA. [Miranda, Felix A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Schwerdt, HN (reprint author), Arizona State Univ, Dept Elect Engn, Tempe, AZ 85287 USA. EM hschwerd@asu.edu FU National Science Foundation [ECCS-0702227]; National Institutes of Health [5R21NS059815-02]; NASA [NNX09AK93H] FX Manuscript received October 15, 2012; revised February 27, 2013; accepted March 01, 2013. Date of publication April 03, 2013; date of current version May 02, 2013. This work was supported in part by the National Science Foundation under Grant ECCS-0702227, the National Institutes of Health under Grant 5R21NS059815-02, and the NASA Graduate Student Research Program under Grant NNX09AK93H. NR 29 TC 12 Z9 12 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 EI 1557-9670 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD MAY PY 2013 VL 61 IS 5 SI SI BP 2170 EP 2176 DI 10.1109/TMTT.2013.2252916 PN 2 PG 7 WC Engineering, Electrical & Electronic SC Engineering GA 141BT UT WOS:000318701100022 ER PT J AU Siegel, PH AF Siegel, Peter H. TI SPECIAL ISSUE ON TERAHERTZ SPECTROSCOPY SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA. [Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAY PY 2013 VL 3 IS 3 SI SI BP 225 EP 227 DI 10.1109/TTHZ.2013.2257191 PG 3 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142BP UT WOS:000318771300001 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Terahertz Pioneers A Series of Interviews With Significant Contributors to Terahertz Science and Technology SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA. [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA. [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA. NR 0 TC 1 Z9 1 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAY PY 2013 VL 3 IS 3 SI SI BP 228 EP 228 DI 10.1109/TTHZ.2013.2256391 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142BP UT WOS:000318771300002 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Terahertz Pioneers: Manfred Winnewisser and Brenda Pruden Winnewisser "Equating Hamiltonians to Nature" SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material ID RESOLUTION INFRARED SPECTRUM; MILLIMETER WAVE SPECTROSCOPY; MOLECULAR QUASI-LINEARITY; ROTATIONAL SPECTRUM; VIBRATION SPECTRUM; LINE-INTENSITIES; GROUND-STATE; HCNO; CARBODIIMIDE; CYANAMIDE C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA. [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA. [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA. EM phs@caltech.edu NR 62 TC 0 Z9 0 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAY PY 2013 VL 3 IS 3 SI SI BP 229 EP 236 DI 10.1109/TTHZ.2013.2256392 PG 8 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142BP UT WOS:000318771300003 ER PT J AU Jepsen, PU Cooke, DG Siegel, PH AF Jepsen, Peter Uhd Cooke, David G. Siegel, Peter H. TI Introduction to the Special Issue on Terahertz Spectroscopy SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Editorial Material C1 [Jepsen, Peter Uhd] Tech Univ Denmark, DTU Foton, DK-2800 Lyngby, Denmark. [Cooke, David G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA. [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Jepsen, PU (reprint author), Tech Univ Denmark, DTU Foton, DK-2800 Lyngby, Denmark. RI Cooke, David/A-7360-2008; OI Jepsen, Peter Uhd/0000-0003-3915-1167 NR 0 TC 3 Z9 3 U1 0 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAY PY 2013 VL 3 IS 3 SI SI BP 237 EP 238 DI 10.1109/TTHZ.2013.2257192 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142BP UT WOS:000318771300004 ER PT J AU Drouin, BJ Pearson, JC Yu, SS Gupta, H AF Drouin, Brian J. Pearson, John C. Yu, Shanshan Gupta, Harshal TI Characterization and Use of a 1.3-1.5 THz Multiplier Chain for Molecular Spectroscopy SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Methanol; molecular spectroscopy; sulfur hydride; THz source characterization ID LAMBDA-DOUBLING SPECTRUM; ROTATIONAL SPECTRUM; SH; METHANOL; STATES; SD; OH AB Modular fixed-tuned wide-bandwidth multiplier sources for THz generation have enabled and greatly simplified high sensitivity molecular spectroscopic measurements. However, the multiplied sources must be carefully characterized. Characterization requires band-wide measurements of power levels and harmonic content, as well as understanding any spurious behavior. Also, simple bias schemes, and acceptable input power levels that eliminate spurious behavior, support long term reliability, and result in repeatable performance are critical in spectroscopic applications. The fully characterized source may then be useful for both narrow-band high sensitivity integrations, or for band-wide surveys. Coupling the source with various gas-handling systems enables valuable new spectroscopic measurements that improve upon techniques such as Tunable Far-Infrared spectroscopy, Laser-sideband spectroscopy, and photomixer based spectroscopy. C1 [Drouin, Brian J.; Pearson, John C.; Yu, Shanshan; Gupta, Harshal] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brian.j.drouin@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU National Aeronautics and Space Administration FX The authors would like to thank E. Cohen for his insight on the magnetic and electric field effects in spectra of radicals. This paper presents research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 20 TC 9 Z9 9 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD MAY PY 2013 VL 3 IS 3 SI SI BP 314 EP 321 DI 10.1109/TTHZ.2013.2255915 PG 8 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142BP UT WOS:000318771300013 ER PT J AU Hsu, SY Cheng, RB AF Hsu, Su-Yuen Cheng, Ron-Bin TI Modeling geometry and progressive interfacial damage in textile composites SO JOURNAL OF COMPOSITE MATERIALS LA English DT Article DE Textile composite material; geometry; interface; progressive damage; meso-mechanical analysis; finite element; cohesive model; contact ID 2X2 BRAIDED COMPOSITES; PLAIN WEAVE COMPOSITES; WOVEN COMPOSITES; ELEMENT-ANALYSIS; FAILURE ANALYSIS; MECHANICS; CELL AB A procedure combining geometrically nonlinear, explicit dynamic contact analysis, computer-aided-design techniques, elasticity-based mesh deformation, and cohesive contact modeling is proposed to efficiently construct practical finite element models for meso-mechanical analysis of progressive damage in textile composites. In the procedure, the geometry of the fiber tows is computed by imposing a fictitious expansion on the tows. Meshes resulting from the procedure are incongruent at the computed tow-tow and tow-matrix interfaces. The interfaces are treated as cohesive contact surfaces not only to resolve the incongruence but also to simulate progressive interfacial damage. Example meshes are constructed for two plain weaves, a ceramic-matrix composite with matrix porosity and a polymeric-matrix composite without porosity. To verify the meshes and interfaces, the composite models are simplified to only have interfacial damage in numerical experiments of uniaxial cyclic loading. Although the computed progression of damage is rather complex, anticipated major qualitative characteristics are reproduced in the computations. C1 [Hsu, Su-Yuen] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Cheng, Ron-Bin] Dassault Syst Simulia Corp, Warwick, RI USA. RP Hsu, SY (reprint author), NASA, Langley Res Ctr, MS 190, Hampton, VA 23681 USA. EM su-yuen.hsu-1@nasa.gov FU Hypersonics Project of the NASA Fundamental Aeronautics Program FX This paper is based on research funded by the Hypersonics Project of the NASA Fundamental Aeronautics Program during 2009 and 2010. NR 25 TC 0 Z9 0 U1 3 U2 24 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-9983 J9 J COMPOS MATER JI J. Compos Mater. PD MAY PY 2013 VL 47 IS 11 BP 1343 EP 1356 DI 10.1177/0021998312447207 PG 14 WC Materials Science, Composites SC Materials Science GA 144PY UT WOS:000318953100003 ER PT J AU Horstmann, M Humayun, M Harries, D Langenhorst, F Chabot, NL Bischoff, A Zolensky, ME AF Horstmann, Marian Humayun, Munir Harries, Dennis Langenhorst, Falko Chabot, Nancy L. Bischoff, Addi Zolensky, Michael E. TI Wustite in the fusion crust of Almahata Sitta sulfide-metal assemblage MS-166: Evidence for oxygen in metallic melts SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DEFECT STRUCTURE; IRON-METEORITES; FE1-XO; CHONDRITE; ELEMENT; OXIDATION; BRECCIA; OXIDE AB Meteorite fusion crusts form during the passage of a meteoroid through the Earth's atmosphere and are highly oxidized intergrowths as documented by the presence of e.g., oxides. The porous and irregular fusion crust surrounding the Almahata Sitta sulfide-metal assemblage MS-166 was found highly enriched in wustite (Fe1-xO). Frictional heating of the outer portions of the assemblage caused partial melting of predominantly the Fe-sulfide and minor amounts of the outer Ni-rich portions of the originally zoned metal in MS-166. Along with melting significant amounts of oxygen were incorporated into the molten fusion crust and mainly FeS was oxidized and desulfurized to form wustite. Considerable amounts of FeS were lost due to ablation, whereas the cores of the large metal grains appear largely unmelted leaving behind metal grains and surrounding wustite-rich material (matte). Metal grains along with the surrounding matte typically form an often highly porous framework of globules interconnected with the matte. Although textures and chemical composition suggest that melting of Fe,Ni metal occurred only partially (Ni-rich rims), there is a trace elemental imprint of siderophile element partitioning influenced by oxygen in the metallic melt as indicated by the behavior of W and Ga, the two elements significantly affected by oxygen in a metallic melt. It is remarkable that MS-166 survived the atmospheric passage as troilite inclusions in iron meteorites are preferentially destroyed. C1 [Horstmann, Marian; Bischoff, Addi] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Humayun, Munir] Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA. [Humayun, Munir] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32310 USA. [Harries, Dennis] Univ Bayreuth, Bayer Geoinst, D-95447 Bayreuth, Germany. [Harries, Dennis; Langenhorst, Falko] Univ Jena, Inst Geowissensch, D-07745 Jena, Germany. [Chabot, Nancy L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Zolensky, Michael E.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. RP Horstmann, M (reprint author), Univ Munster, Inst Planetol, Wilhelm Klemm Str 10, D-48149 Munster, Germany. EM marianhorstmann@uni-muenster.de RI Chabot, Nancy/F-5384-2015; Harries, Dennis/P-1755-2016; OI Chabot, Nancy/0000-0001-8628-3176; Humayun, Munir/0000-0001-8516-9435 FU German Research Foundation (DFG) [SPP 1385]; NASA Cosmochemistry Program [NNX10AI37G, NNX12AH88G] FX Ulla Heitmann (Munster) is acknowledged for sample preparation. M. J. Genge, an anonymous reviewer, and associate editor E. R. D. Scott provided constructive reviews and very helpful comments that significantly improved the manuscript. This work was partly supported by the German Research Foundation (DFG) within the priority program "The First 10 Million Years of the Solar System-A Planetary Materials Approach" (SPP 1385) and by the NASA Cosmochemistry Program through grants NNX10AI37G (M. Humayun) and NNX12AH88G (N. L. Chabot). NR 43 TC 4 Z9 4 U1 1 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD MAY PY 2013 VL 48 IS 5 BP 730 EP 743 DI 10.1111/maps.12097 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 143OP UT WOS:000318877300002 ER PT J AU Cohen, BA AF Cohen, Barbara A. TI The Vestan cataclysm: Impact-melt clasts in howardites and the bombardment history of 4 Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CANYON SANIDINE STANDARD; LATE HEAVY BOMBARDMENT; K-40 DECAY CONSTANTS; HED PARENT BODY; COLLISIONAL HISTORY; AR-40/AR-39 GEOCHRONOLOGY; JOINT DETERMINATION; KAPOETA HOWARDITE; IMPROVED ACCURACY; AR-40-AR-39 AGES AB Crystalline impact-melt samples were created in high-temperature environments by relatively large craters and, as such, give additional constraints on the nature of the impacts that created them. This article provides new 40Ar-39Ar ages of impact-melt clasts in howardites and shows that these clasts formed on the HED parent body, 4 Vesta, within the time period 3.33.8Ga. Rather than resulting from an increased number of impacts, however, impact-melted material in howardites may result from unusually high-velocity impacts occurring in the asteroid belt during this period. This scenario is similar to the late heavy bombardment of the Moon, pointing to an unusual dynamical event at this time across the inner solar system. Therefore, impact-melt rocks in howardites uniquely record a Vestan cataclysm. C1 NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Cohen, BA (reprint author), NASA, Marshall Space Flight Ctr, Mail Code ZP13, Huntsville, AL 35812 USA. EM barbara.a.cohen@nasa.gov FU NASA Cosmochemistry program [NNX07AI57G] FX This manuscript benefited from discussions with Tim Swindle and Simone Marchi, and was strengthened by reviews by Don Bogard and Brad Jolliff. I thank the Meteorite Working Group for their wisdom in allocating the howardite samples despite my request for a lunar breccia. This work was supported by the NASA Cosmochemistry program via grant NNX07AI57G to B. A. Cohen and used the NASA Astrophysical Data System Abstract Service. NR 63 TC 10 Z9 10 U1 2 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD MAY PY 2013 VL 48 IS 5 BP 771 EP 785 DI 10.1111/maps.12101 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 143OP UT WOS:000318877300005 ER PT J AU Callahan, MP Burton, AS Elsila, JE Baker, EM Smith, KE Glavin, DP Dworkin, JP AF Callahan, Michael P. Burton, Aaron S. Elsila, Jamie E. Baker, Eleni M. Smith, Karen E. Glavin, Daniel P. Dworkin, Jason P. TI A search for amino acids and nucleobases in the Martian meteorite Roberts Massif 04262 using liquid chromatography-mass spectrometry SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CARBONACEOUS CHONDRITES; MURCHISON METEORITE; EXTRATERRESTRIAL NUCLEOBASES; ORGANIC-MATTER; PARENT BODY; TG-FTIR; NITROGEN; PYROLYSIS; PATHWAYS; ALH84001 AB The investigation into whether Mars contains signatures of past or present life is of great interest to science and society. Amino acids and nucleobases are compounds that are essential for all known life on Earth and are excellent target molecules in the search for potential Martian biomarkers or prebiotic chemistry. Martian meteorites represent the only samples from Mars that can be studied directly in the laboratory on Earth. Here, we analyzed the amino acid and nucleobase content of the shergottite Roberts Massif (RBT) 04262 using liquid chromatography-mass spectrometry. We did not detect any nucleobases above our detection limit in formic acid extracts; however, we did measure a suite of protein and nonprotein amino acids in hot-water extracts with high relative abundances of -alanine and -amino-n-butyric acid. The presence of only low (to absent) levels of several proteinogenic amino acids and a lack of nucleobases suggest that this meteorite fragment is fairly uncontaminated with respect to these common biological compounds. The distribution of straight-chained amine-terminal n--amino acids in RBT 04262 resembled those previously measured in thermally altered carbonaceous meteorites (Burton etal. 2012; Chan etal. 2012). A carbon isotope ratio of 24 parts per thousand +/- 6 parts per thousand for -alanine in RBT 04262 is in the range of reduced organic carbon previously measured in Martian meteorites (Steele etal. 2012). The presence of n--amino acids may be due to a high temperature Fischer-Tropsch-type synthesis during igneous processing on Mars or impact ejection of the meteorites from Mars, but more experimental data are needed to support these hypotheses. C1 [Callahan, Michael P.; Elsila, Jamie E.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Callahan, Michael P.; Elsila, Jamie E.; Glavin, Daniel P.; Dworkin, Jason P.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Burton, Aaron S.] NASA Postdoctoral Program Administered Oak Ridge, Greenbelt, MD 20771 USA. [Baker, Eleni M.] Bullis Sch, Potomac, MD 20854 USA. [Smith, Karen E.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Smith, Karen E.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. RP Callahan, MP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM michael.p.callahan@nasa.gov RI Elsila, Jamie/C-9952-2012; Callahan, Michael/D-3630-2012; Glavin, Daniel/D-6194-2012; Burton, Aaron/H-2212-2011; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Burton, Aaron/0000-0002-7137-1605; Dworkin, Jason/0000-0002-3961-8997 FU NASA Astrobiology Institute; Goddard Center for Astrobiology; NASA FX The authors thank Cecilia Satterwhite (NASA JSC), Kevin Righter (NASA JSC), and the Meteorite Working Group for providing the Martian meteorites. M. P. C., J. E. E., D. P. G., and J. P. D. acknowledge funding support from the NASA Astrobiology Institute and The Goddard Center for Astrobiology and the NASA Cosmochemistry Program. A. S. B. acknowledges support from the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. We also thank H. James Cleaves II for helpful comments and discussions of this manuscript. NR 46 TC 17 Z9 17 U1 3 U2 50 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD MAY PY 2013 VL 48 IS 5 BP 786 EP 795 DI 10.1111/maps.12103 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 143OP UT WOS:000318877300006 ER PT J AU McCubbin, FM Elardo, SM Shearer, CK Smirnov, A Hauri, EH Draper, DS AF McCubbin, Francis M. Elardo, Stephen M. Shearer, Charles K., Jr. Smirnov, Alexander Hauri, Erik H. Draper, David S. TI A petrogenetic model for the comagmatic origin of chassignites and nakhlites: Inferences from chlorine-rich minerals, petrology, and geochemistry SO METEORITICS & PLANETARY SCIENCE LA English DT Review ID SULFUR ISOTOPIC COMPOSITIONS; HOSTED MELT INCLUSIONS; PHYRIC MARTIAN BASALTS; RARE-EARTH-ELEMENTS; RAY EXPOSURE AGES; OXYGEN FUGACITY; OXIDATION-STATE; LAYERED INTRUSIONS; UPPER-MANTLE; EARLY DIFFERENTIATION AB Twelve samples belonging to the chassignite and nakhlite subgroups of Martian meteorites were investigated using a variety of micro-beam analytical techniques to gain insight into the petrogenesis of these two meteorite classes. There are a striking number of geochemical similarities between the chassignites and nakhlites, including mineralogy and petrology, crystallization age, cosmic-ray exposure age, and radiogenic isotopic compositions. However, there are also geochemical differences, namely in trace element systematics of pyroxenes, that have led some authors to conclude that the nakhlites are comagmatic with each other, but not comagmatic with the chassignites. On the basis of data presented here, we propose a model in which these differences can be reconciled by the addition of an exogenous Cl-rich fluid to the chassignite-nakhlite magma body shortly after the formation of the cumulate horizon that was sampled by the Chassigny meteorite. This model is supported by the textural and chemical associations of the volatile-bearing minerals apatite, amphibole, and biotite, which record a history starting with the addition of a Cl- and LREE-enriched fluid to the magma body. As the magma continued to crystallize, it eventually reached chloride saturation and degassed a Cl-rich fluid phase. Depending on the provenance of the Cl-rich fluid, this model could explain how the chassignites and nakhlites originated from an LREE-depleted source, yet all exhibit LREE-enriched bulk-rock patterns. Additionally, the model explains the range in oxygen fugacity that is recorded by the chassignites and nakhlites because eventual exsolution and loss of Cl-rich fluid phases near the end of crystallization of the nakhlite sequence leads to auto-oxidation of the magma body due to the preferential partitioning of Fe2+ into the fluid phase. C1 [McCubbin, Francis M.; Elardo, Stephen M.; Shearer, Charles K., Jr.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Smirnov, Alexander] Dowling Coll, Dept Earth & Marine Sci, Oakdale, NY 11769 USA. [Hauri, Erik H.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Draper, David S.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP McCubbin, FM (reprint author), Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. EM fmccubbi@unm.edu RI Elardo, Stephen/E-5865-2010; McCubbin, Francis/D-1698-2009; Smirnov, Alexander/D-4672-2009 OI Smirnov, Alexander/0000-0001-8665-5187 FU NASA [NNX11AG76G, NNX10AI77G, NNX12AO15H, NNX08AH81G]; New Mexico Space Grant Consortium FX We thank the reviewers Lydia Hallis, Justin Filiberto, and James Day for very insightful and helpful comments that greatly improved the quality of the manuscript. We also thank Christine Floss for all of her effort as Associate Editor. We thank Hanna Nekvasil, Donald Lindsley, Aaron Bell, and James Papike for helpful discussions on the topic of this manuscript. This work was funded by NASA Cosmochemistry grants NNX11AG76G to F. M. M. and NNX10AI77G to C. K. S. Additionally, S. M. E. gratefully acknowledges support from NASA Earth and Space Science Fellow NNX12AO15H, Cosmochemistry grant NNX08AH81G to D. S. D., and a graduate fellowship from the New Mexico Space Grant Consortium during this study. NR 238 TC 51 Z9 51 U1 3 U2 44 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 MAY PY 2013 VL 48 IS 5 BP 819 EP 853 DI 10.1111/maps.12095 PG 35 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 143OP UT WOS:000318877300009 ER PT J AU De Gregorio, BT Stroud, RM Nittler, LR Alexander, CMO Bassim, ND Cody, GD Kilcoyne, ALD Sandford, SA Milam, SN Nuevo, M Zega, TJ AF De Gregorio, Bradley T. Stroud, Rhonda M. Nittler, Larry R. Alexander, Conel M. O'D Bassim, Nabil D. Cody, George D. Kilcoyne, A. L. David Sandford, Scott A. Milam, Stefanie N. Nuevo, Michel Zega, Thomas J. TI Isotopic and chemical variation of organic nanoglobules in primitive meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INTERPLANETARY DUST PARTICLES; TAGISH LAKE METEORITE; CARBONACEOUS CHONDRITES; MURCHISON METEORITE; SOLAR-SYSTEM; INTERSTELLAR CHEMISTRY; AROMATIC-HYDROCARBONS; PRESOLAR GRAPHITE; NITROGEN ISOTOPE; N-14/N-15 RATIO AB Organic nanoglobules are microscopic spherical carbon-rich objects present in chondritic meteorites and other astromaterials. We performed a survey of the morphology, organic functional chemistry, and isotopic composition of 184 nanoglobules in insoluble organic matter (IOM) residues from seven primitive carbonaceous chondrites. Hollow and solid nanoglobules occur in each IOM residue, as well as globules with unusual shapes and structures. Most nanoglobules have an organic functional chemistry similar to, but slightly more carboxyl-rich than, the surrounding IOM, while a subset of nanoglobules have a distinct, highly aromatic functionality. The range of nanoglobule N isotopic compositions was similar to that of nonglobular 15N-rich hotspots in each IOM residue, but nanoglobules account for only about one third of the total 15N-rich hotspots in each sample. Furthermore, many nanoglobules in each residue contained no 15N enrichment above that of bulk IOM. No morphological indicators were found to robustly distinguish the highly aromatic nanoglobules from those that have a more IOM-like functional chemistry, or to distinguish 15N-rich nanoglobules from those that are isotopically normal. The relative abundance of aromatic nanoglobules was lower, and nanoglobule diameters were greater, in more altered meteorites, suggesting the creation/modification of IOM-like nanoglobules during parent-body processing. However, 15N-rich nanoglobules, including many with highly aromatic functional chemistry, likely reflect preaccretionary isotopic fractionation in cold molecular cloud or protostellar environments. These data indicate that no single formation mechanism can explain all of the observed characteristics of nanoglobules, and their properties are likely a result of multiple processes occurring in a variety of environments. C1 [De Gregorio, Bradley T.] Nova Res Inc, Alexandria, VA 22308 USA. [De Gregorio, Bradley T.; Stroud, Rhonda M.; Bassim, Nabil D.] USN, Res Lab, Mat Sci & Technol Div, Washington, DC 20375 USA. [Nittler, Larry R.; Alexander, Conel M. O'D] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Cody, George D.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Kilcoyne, A. L. David] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Sandford, Scott A.; Nuevo, Michel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Milam, Stefanie N.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nuevo, Michel] SETI Inst, Mountain View, CA 94043 USA. [Zega, Thomas J.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP De Gregorio, BT (reprint author), Nova Res Inc, Alexandria, VA 22308 USA. EM bradley.degregorio.ctr@nrl.navy.mil RI Milam, Stefanie/D-1092-2012; Alexander, Conel/N-7533-2013; De Gregorio, Bradley/B-8465-2008; Kilcoyne, David/I-1465-2013; Stroud, Rhonda/C-5503-2008 OI Milam, Stefanie/0000-0001-7694-4129; Alexander, Conel/0000-0002-8558-1427; De Gregorio, Bradley/0000-0001-9096-3545; Stroud, Rhonda/0000-0001-5242-8015 FU Office of Naval Research, NASA; NASA Astrobiology Institute; U.S. Department of Energy; Natural Sciences and Engineering Research Council of Canada; National Research Council Canada; Canadian Institutes of Health Research; Province of Saskatchewan, Western Economic Diversification Canada; University of Saskatchewan FX We sincerely thank Drs. L. Remusat, G. Matrajt, N. Johnson, and associate editor C. Floss for their constructive reviews. This work was supported by the Office of Naval Research, NASA Cosmochemistry and Origins of Solar Systems Programs, and the NASA Astrobiology Institute. This research was conducted while the primary author held a National Research Council Research Associateship at the U.S. Naval Research Laboratory. Use of the Advanced Light Source was supported by the U.S. Department of Energy. Use of the Canadian Light Source was supported by the Natural Sciences and Engineering Research Council of Canada, the National Research Council Canada, the Canadian Institutes of Health Research, the Province of Saskatchewan, Western Economic Diversification Canada, and the University of Saskatchewan. NR 98 TC 15 Z9 15 U1 1 U2 28 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 MAY PY 2013 VL 48 IS 5 BP 904 EP 928 DI 10.1111/maps.12109 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 143OP UT WOS:000318877300013 ER PT J AU Dempsey, PJ Sheng, SW AF Dempsey, Paula J. Sheng, Shuangwen TI Investigation of data fusion applied to health monitoring of wind turbine drivetrain components SO WIND ENERGY LA English DT Article DE data fusion; health monitoring; oil-debris analysis; vibration analysis; wind turbine drivetrain AB The research described was performed with diagnostic tools used to detect damage to dynamic mechanical components in a wind turbine gearbox. Different monitoring technologies were evaluated by collecting vibration and oil-debris data from tests performed on both a healthy' gearbox and a damaged gearbox that were mounted on a dynamometer test stand at the National Renewable Energy Laboratory (NREL). The damaged gearbox tested had been removed from the field after it experienced component damage because of two events that resulted in the loss of oil. The gearbox was re-tested under controlled conditions by using the NREL dynamometer test stand. Preliminary results indicate that oil-debris and vibration data can be integrated to improve the assessment of the health of the wind turbine gearbox. Copyright (c) 2012 John Wiley & Sons, Ltd. C1 [Dempsey, Paula J.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Sheng, Shuangwen] Natl Renewable Energy Lab, Golden, CO 80401 USA. RP Sheng, SW (reprint author), Natl Renewable Energy Lab, Golden, CO 80401 USA. EM Shuangwen.Sheng@nrel.gov OI sheng, shuangwen/0000-0003-0134-0907 FU US Department of Energy; NREL FX The authors thank the US Department of Energy for its support of this work. We also acknowledge and appreciate the support given by the NREL condition-monitoring partners. NR 17 TC 5 Z9 6 U1 1 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1095-4244 J9 WIND ENERGY JI Wind Energy PD MAY PY 2013 VL 16 IS 4 BP 479 EP 489 DI 10.1002/we.1512 PG 11 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA 145LR UT WOS:000319018100001 ER PT J AU Yang, F Coughlin, DR Phillips, PJ Yang, L Devaraj, A Kovarik, L Noebe, RD Mills, MJ AF Yang, F. Coughlin, D. R. Phillips, P. J. Yang, L. Devaraj, A. Kovarik, L. Noebe, R. D. Mills, M. J. TI Structure analysis of a precipitate phase in an Ni-rich high-temperature NiTiHf shape memory alloy SO ACTA MATERIALIA LA English DT Article DE Shape memory alloys (SMAs); Precipitation; Crystal structure; High-angle annular dark field (HAADF); Ab initio electron theory ID TOTAL-ENERGY CALCULATIONS; WAVE BASIS-SET; MARTENSITIC-TRANSFORMATION; ULTRASOFT PSEUDOPOTENTIALS; MICROSTRUCTURE; TRANSITION; SIMULATION; STEM AB Thermal aging of the high-temperature shape memory alloy 50.3Ni-29.7Ti-20Hf (at.%) introduces a novel precipitate phase that plays an important role in improving shape memory properties. The precipitate phase was investigated by conventional electron diffraction, high-resolution scanning transmission electron microscopy (STEM) and three-dimensional atom probe tomography. An unrelaxed orthorhombic atomic structural model is proposed based on these observations. This model was subsequently relaxed by ab initio calculations. As a result of the relaxation, atom shuffle displacements occur, which in turn yields improved agreement with the STEM images. The relaxed structure, which is termed the "H phase", has also been verified to be thermodynamically stable at 0 K. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Yang, F.; Coughlin, D. R.; Yang, L.; Mills, M. J.] Ohio State Univ, Columbus, OH 43210 USA. [Phillips, P. J.] Univ Illinois, Chicago, IL 60608 USA. [Devaraj, A.; Kovarik, L.] Pacific NW Natl Lab, Richland, WA 99354 USA. [Noebe, R. D.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Yang, F (reprint author), Ohio State Univ, Columbus, OH 43210 USA. EM yang.1052@osu.edu RI Mills, Michael/I-6413-2013; Kovarik, Libor/L-7139-2016 FU US Department of Energy, Office of Basic Energy Sciences [DE-SC0001258]; NASA Fundamental Aeronautics Program, Supersonics Project, Dale Hopkins, API; DOE's Office of Biological and Environmental Research; DOE [DE-AC05-76RLO1830] FX This work was supported by the US Department of Energy, Office of Basic Energy Sciences under Grant #DE-SC0001258 (for F.Y. and M.J.M.). R.D.N. acknowledges funding from the NASA Fundamental Aeronautics Program, Supersonics Project, Dale Hopkins, API. A part of this work was conducted in the William R. Wiley Environmental Molecular Sciences Laboratory (EMSL), a national scientific user facility sponsored by DOE's Office of Biological and Environmental Research and located at PNNL. PNNL is operated by Battelle for the DOE under Contract DE-AC05-76RLO1830. NR 25 TC 37 Z9 38 U1 4 U2 53 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 MAY PY 2013 VL 61 IS 9 BP 3335 EP 3346 DI 10.1016/j.actamat.2013.02.023 PG 12 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 138TS UT WOS:000318533500020 ER PT J AU Beaudoin, AJ Obstalecki, M Tayon, W Hemquist, M Mudrock, R Kenesei, P Lienert, U AF Beaudoin, A. J. Obstalecki, M. Tayon, W. Hemquist, M. Mudrock, R. Kenesei, P. Lienert, U. TI In situ assessment of lattice strain in an Al-Li alloy SO ACTA MATERIALIA LA English DT Article DE Synchrotron diffraction; In situ tension test; Material properties; Aluminum alloy ID ALUMINUM-LITHIUM ALLOYS; FRACTURE; ANISOTROPY; DEFORMATION; ORIENTATION; TOUGHNESS; BEHAVIOR; FATIGUE; SPACE; BULK AB The lattice strains of individual grains are measured in an Al-Li alloy, AA 2195, using high-energy X-ray diffraction at a synchrotron source. The diffraction of individual grains in this highly textured production alloy was isolated through use of a depth-defining aperture. It is shown that hydrostatic stress, and in turn the stress triaxiality, can vary significantly from grain to grain. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Beaudoin, A. J.] Univ Illinois, Urbana, IL 61801 USA. [Obstalecki, M.] Cornell Univ Ithaca, Ithaca, NY USA. [Tayon, W.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Hemquist, M.] Northrop Grumman, Azusa, CA USA. [Mudrock, R.] Honeywell, Des Plaines, IL USA. [Kenesei, P.] Argonne Natl Lab, Adv Photon Source, Argonne, IL 60439 USA. [Lienert, U.] Deutsch Elektronen Synchrotron DESY, Hamburg, Germany. RP Beaudoin, AJ (reprint author), Univ Illinois, 1206 West Green St, Urbana, IL 61801 USA. EM abeaudoi@illinois.edu; mo362@-comell.edu; wesley.a.tayon@nasa.gov; mark.hemquist@gmail.com; rstorer87@gmail.com; kenesei@aps.anl.gov; ulrich.lienert@desy.de FU NASA [NNX09AN21G]; US Department of Energy [DEFG36-05GO15049]; US Department of Energy, Office of Science, Office of Basic Energy Sciences, [DE-AC02-06CH11357] FX This work was supported by NASA under Contract No. NNX09AN21G and the US Department of Energy under Contract No. DEFG36-05GO15049. Use of the Advanced Photon Source was supported by the US Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-06CH11357. Ms. Katherine Halm assisted in the HEDM experiment and Dr. Roy Crooks aided in collection of the EBSD images. Drs. Jette Oddershede, Soren Schmidt and Jon Wright provided assistance in use of the Fable suite of analysis programs. Conversations with Doug Wells and Preston McGill of the Marshall Spaceflight Center offered guidance to our studies of Al-Li alloys. We also thank Dr. Roberto Rioja for comments and directing us to Ref. [18]. NR 32 TC 12 Z9 13 U1 5 U2 41 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 EI 1873-2453 J9 ACTA MATER JI Acta Mater. PD MAY PY 2013 VL 61 IS 9 BP 3456 EP 3464 DI 10.1016/j.actamat.2013.02.037 PG 9 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 138TS UT WOS:000318533500031 ER PT J AU Kukavskaya, EA Soja, AJ Petkov, AP Ponomarev, EI Ivanova, GA Conard, SG AF Kukavskaya, Elena A. Soja, Amber J. Petkov, Alexander P. Ponomarev, Evgeni I. Ivanova, Galina A. Conard, Susan G. TI Fire emissions estimates in Siberia: evaluation of uncertainties in area burned, land cover, and fuel consumption SO CANADIAN JOURNAL OF FOREST RESEARCH-REVUE CANADIENNE DE RECHERCHE FORESTIERE LA English DT Article ID FOREST-FIRES; NORTHERN EURASIA; BOREAL FORESTS; CARBON BUDGET; MODIS; PRODUCTS; RUSSIA; ATMOSPHERE; ALGORITHM; CLIMATE AB Boreal forests constitute the world's largest terrestrial carbon pools. The main natural disturbance in these forests is wildfire, which modifies the carbon budget and atmosphere, directly and indirectly. Wildfire emissions in Russia contribute substantially to the global carbon cycle and have potentially important feedbacks to changing climate. Published estimates of carbon emissions from fires in Russian boreal forests vary greatly depending on the methods and data sets used. We examined various fire and vegetation products used to estimate wildfire emissions for Siberia. Large (up to fivefold) differences in annual and monthly area burned estimates for Siberia were found among four satellite-based fire data sets. Official Russian data were typically less than 10% of satellite estimates. Differences in the estimated proportion of annual burned area within each ecosystem were as much as 40% among five land-cover products. As a result, fuel consumption estimates would be expected to vary widely (3%-98%) depending on the specific vegetation mapping product used and as a function of weather conditions. Verification and validation of burned area and land-cover data sets along with the development of fuel maps and combustion models are essential for accurate Siberian wildfire emission estimates, which are central to balancing the carbon budget and assessing feedbacks to climate change. C1 [Kukavskaya, Elena A.; Ponomarev, Evgeni I.; Ivanova, Galina A.] VN Sukachev Inst Forest SB RAS, Krasnoyarsk 660036, Russia. [Soja, Amber J.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Soja, Amber J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Petkov, Alexander P.; Conard, Susan G.] US Forest Serv, USDA, Rocky Mt Res Stn, Missoula, MT 59808 USA. [Conard, Susan G.] George Mason Univ, Fairfax, VA 22030 USA. RP Kukavskaya, EA (reprint author), VN Sukachev Inst Forest SB RAS, Akademgorodok 50-28, Krasnoyarsk 660036, Russia. EM kukavskaya@ksc.krasn.ru RI Conard, Susan/H-8158-2013; Evgenii, Ponomarev/A-7595-2013; Kukavskaya, Elena/I-8155-2014 OI Evgenii, Ponomarev/0000-0002-7185-3639; FU National Aeronautics and Space Administration (NASA); Land Cover Land Use Change (LCLUC) project under Northern Eurasia Earth Science Partnership Initiative (NEESPI); Terrestrial Ecology (TE) project under Northern Eurasia Earth Science Partnership Initiative (NEESPI); Inter-DiSciplinary (IDS) project under Northern Eurasia Earth Science Partnership Initiative (NEESPI); Institute of International Education, Fulbright Scholar Program; Russian Foundation for Basic Research [12-04-31258]; FGP "Scientific and scientific-pedagogical staff of innovative Russia"; Russian Academy of Sciences FX The authors gratefully acknowledge financial support from the National Aeronautics and Space Administration (NASA), Land Cover Land Use Change (LCLUC), Terrestrial Ecology (TE), and Inter-DiSciplinary (IDS) projects, all of which fall under the Northern Eurasia Earth Science Partnership Initiative (NEESPI) domain; the Institute of International Education, Fulbright Scholar Program; the Russian Foundation for Basic Research (Grant No. 12-04-31258; FGP "Scientific and scientific-pedagogical staff of innovative Russia"; and the Russian Academy of Sciences. NR 65 TC 14 Z9 17 U1 1 U2 24 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0045-5067 EI 1208-6037 J9 CAN J FOREST RES JI Can. J. For. Res.-Rev. Can. Rech. For. PD MAY PY 2013 VL 43 IS 5 BP 493 EP 506 DI 10.1139/cjfr-2012-0367 PG 14 WC Forestry SC Forestry GA 142GL UT WOS:000318785100008 ER PT J AU Amediek, A Sun, XL Abshire, JB AF Amediek, Axel Sun, Xiaoli Abshire, James B. TI Analysis of Range Measurements From a Pulsed Airborne CO2 Integrated Path Differential Absorption Lidar SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Carbon dioxide; integrated path differential absorption (IPDA); lidar; ranging ID ATMOSPHERIC CO2; LASER ALTIMETERS; CARBON-DIOXIDE; MODELS AB Determining the CO2 column abundance from an integrated path differential absorption (IPDA) lidar requires accurate knowledge of the range to the scattering surface, i.e., the column height. We have adapted and tested a ranging algorithm for the airborne IPDA CO2 lidar designed at the NASA Goddard Space Flight Center, and have evaluated its accuracy and precision. We applied a quasi-maximum-likelihood method, using cross correlation, to estimate the range from the lidar's 1-mu s-wide echo pulses. The objective was to show that the use of these temporally long laser pulses allows the determination of the optical path length with required precision. We analyzed airborne measurements made in August 2009 over the Chesapeake Bay near the Eastern Shore of Virginia. The results indicate a ranging precision of better than 3 m, which is sufficient for airborne and space-based retrievals of CO2 column concentration. C1 [Amediek, Axel] Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atmosphare, D-82234 Wessling, Germany. [Sun, Xiaoli; Abshire, James B.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Amediek, A (reprint author), Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atmosphare, D-82234 Wessling, Germany. EM axel.amediek@dlr.de; xiaoli.sun-1@nasa.gov; james.b.abshire@nasa.gov RI Abshire, James/I-2800-2013; Sun, Xiaoli/B-5120-2013 FU National Aeronautics and Space Administration (NASA) Earth Science Technology Office's Instrument Incubator Program; NASA; Goddard Space Flight Center Internal Research and Development program; German Aerospace Center (DLR) under Forschungssemester Grant FX This work was supported in part by the National Aeronautics and Space Administration (NASA) Earth Science Technology Office's Instrument Incubator Program, by the NASA Active Sensing of CO2 Emission Over Nights, Days, and Seasons Definition Program, and by the Goddard Space Flight Center Internal Research and Development program. The work of A. Amediek was supported by the German Aerospace Center (DLR) under Forschungssemester Grant. NR 19 TC 5 Z9 6 U1 3 U2 18 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAY PY 2013 VL 51 IS 5 BP 2498 EP 2504 DI 10.1109/TGRS.2012.2216884 PN 1 PG 7 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 137IJ UT WOS:000318428700002 ER PT J AU Rault, DF Loughman, RP AF Rault, Didier F. Loughman, Robert P. TI The OMPS Limb Profiler Environmental Data Record Algorithm Theoretical Basis Document and Expected Performance SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Atmospheric ozone vertical distribution; limb scatter (LS); remote sensing ID SOLAR MESOSPHERE EXPLORER; ALGEBRAIC RECONSTRUCTION TECHNIQUE; STRATOSPHERIC OZONE PROFILES; RADIATIVE-TRANSFER MODEL; SCATTER MEASUREMENTS; OSIRIS INSTRUMENT; VERTICAL PROFILES; SPECTRAL REGION; ODIN SATELLITE; O-3 PROFILES AB The retrieval algorithm for the Suomi National Polar-Orbiting Partnership (NPP) Ozone Mapping and Profiler Suite (OMPS) Limb Profiler is described. The goal of the OMPS Limb Profiler is to produce high quality vertical profiles of ozone in the stratosphere and upper troposphere. Additional products include aerosol extinction vertical profiles together with an estimate of the Angstrom coefficient, cloud top height and NO 2 column density. The ozone retrieval algorithm relies on the optimal estimation approach, and uses the Pair/Triplet methodology. Estimates of bias and random errors are presented, together with a brief description of the operational code output products and the planned validation. C1 [Rault, Didier F.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Loughman, Robert P.] Hampton Univ, Hampton, VA 23668 USA. RP Rault, DF (reprint author), NASA, Univ Space Res Assoc, Goddard Earth Sci Technol & Res Program, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM didier.f.rault@nasa.gov; robert.loughman@hamptonu.edu NR 88 TC 10 Z9 10 U1 0 U2 11 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 MAY PY 2013 VL 51 IS 5 BP 2505 EP 2527 DI 10.1109/TGRS.2012.2213093 PN 1 PG 23 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 137IJ UT WOS:000318428700003 ER PT J AU Broaden, A Zhang, TX Edwards, VM Tan, A Winebarger, A Zhang, J Wu, ST AF Broaden, A. Zhang, T. X. Edwards, V. M. Tan, A. Winebarger, A. Zhang, Jun Wu, S. T. TI The role of electromagnetic ion-cyclotron waves in solar He-3-rich events SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Solar energetic particle; Solar flare; Solar corona; Plasma wave ID ENERGETIC PARTICLE EVENTS; SELECTIVE ACCELERATION; MAGNETIC TOPOLOGY; ULTRAHEAVY IONS; X-RAY; FLARES; HEAVY; PLASMA; HE-3; ENHANCEMENTS AB The preferential heating of He-3 by the electromagnetic ion-cyclotron waves, which propagate in the direction parallel to the magnetic fields in the solar corona, is investigated. The results obtained from this study indicate that the parallel propagating electromagnetic ion-cyclotron waves, if driven, can be efficient at heating He-3 through the first harmonic resonance. This preferential heating of He-3 can lead to a high temperature ratio T-3He/T-4He similar to 10-20 and thus largely increases the number of He-3 to be further accelerated to high energies. Comparing to the electrostatic ion-cyclotron waves, we find that the electromagnetic ion-cyclotron waves can be even more efficient at heating He-3 than the electrostatic ion-cyclotron waves if both types of waves are excited with comparable wave energy densities. Therefore, the electromagnetic ion-cyclotron waves, if generated in solar flares, should also play an important role in solar He-3-rich events along with the electrostatic ion-cyclotron waves. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Broaden, A.; Zhang, T. X.; Edwards, V. M.; Tan, A.] Alabama A&M Univ, Normal, AL 35762 USA. [Winebarger, A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Zhang, Jun] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China. [Wu, S. T.] Univ Alabama, Huntsville, AL 35899 USA. RP Zhang, TX (reprint author), Alabama A&M Univ, Normal, AL 35762 USA. EM tianxi.zhang@aamu.edu FU NASA EPSCoR [NNX07AL52A]; National Natural Science Foundation of China [G40890161]; NSF REU; NSF CISM; Alabama AM University FX This work was supported by NASA EPSCoR grant (NNX07AL52A), National Natural Science Foundation of China (G40890161), NSF REU program, and NSF CISM research program, and Alabama A&M University Title III program. T.X.Z. is indebted to Dr. M. Edwards and Dr. M. Aggarwal for support. NR 42 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 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD MAY PY 2013 VL 97 BP 22 EP 28 DI 10.1016/j.jastp.2013.02.009 PG 7 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 140PJ UT WOS:000318667100003 ER PT J AU Ngwira, CM Seemala, GK Habarulema, JB AF Ngwira, Chigomezyo M. Seemala, Gopi K. Habarulema, John Bosco TI Simultaneous observations of ionospheric irregularities in the African low-latitude region SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Geomagnetic storms; Ionosphere; Total electron content; Equatorial irregularities; Plasma bubbles; Penetration electric field; Equatorial counter-electrojet ID TOTAL ELECTRON-CONTENT; F-LAYER IRREGULARITIES; EQUATORIAL SPREAD-F; MAGNETOSPHERIC DISTURBANCES; MAGNETIC STORMS; GPS; SCINTILLATIONS; SATELLITE; SYSTEM; FIELDS AB Ionospheric storms represent large global disturbances of the ionospheric F-region electron density in response to geomagnetic storms. This study investigates the ionospheric response during a minor geomagnetic storm that occurred on 13-15 September 2004. In particular, we use total electron content (TEC) measurements (rate of TEC change, ROT) to examine the presence of ionospheric irregularities over four low-latitude stations in the African sector, a region that has been less studied. Ionospheric irregularities are known to cause fading and phase fluctuation of L-band radio navigation signals such as those used by the Global Navigation Satellite Systems (GNSS), and are a common feature in the equatorial and low-latitude ionosphere. In the present study, the storm began with a sudden commencement at approximately 20:00 UT on 13 September, while the peak of the main phase occurred on 14 September with an SYM-H index value around -59 nT. On 13 September, the storm did not appear to hinder the development of irregularities as they were observed over all the stations. In contrast, irregularities were rarely observed at two of the 4 stations under study and were absent over the other two stations on 14 September. The DSMP F15 satellite post-sunset flight over the African region observed deep density depletions on 13 September that can be associated with the presence of ionospheric plasma bubble irregularities. Furthermore, an analysis of Delta H (horizontal geomagnetic component corrected for ring current effects) shows that there was a strong positive Delta H perturbation observed in the post-sunset hours on 13 September, which suggests the presence of an eastward penetration electric field, while a negative perturbation of Delta H, which is associated with the equatorial counter-electrojet, was observed on 14 September. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ngwira, Chigomezyo M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Ngwira, Chigomezyo M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Seemala, Gopi K.] Res Inst Sustainable Humanosphere, Kyoto 6110011, Japan. [Habarulema, John Bosco] South African Natl Space Agcy SANSA Space Sci, ZA-7200 Hermanus, South Africa. RP Ngwira, CM (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM chigomezyo.ngwira@nasa.gov RI ngwira, chigomezyo/D-7310-2012; Seemala, Gopi/J-7050-2012; OI Seemala, Gopi/0000-0002-3690-7873; Habarulema, John Bosco/0000-0002-9716-7688 NR 41 TC 13 Z9 13 U1 1 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD MAY PY 2013 VL 97 BP 50 EP 57 DI 10.1016/j.jastp.2013.02.014 PG 8 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 140PJ UT WOS:000318667100007 ER PT J AU Chan, MA Comiso, JC AF Chan, Mark Aaron Comiso, Josefino C. TI Arctic Cloud Characteristics as Derived from MODIS, CALIPSO, and CloudSat SO JOURNAL OF CLIMATE LA English DT Article ID SEA-ICE; PART I; TEMPERATURE; ALGORITHM; SURFACE; DEPTH AB The Moderate Resolution Imaging Spectroradiometer (MODIS), Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP), and CloudSat Cloud Profiling Radar (CPR) set of sensors, all in the Afternoon Constellation (A-Train), has been regarded as among the most powerful tools for characterizing the cloud cover. While providing good complementary information, the authors also observed that, at least for the Arctic region, the different sensors provide significantly different statistics about cloud cover characteristics. Data in 2007 and 2010 were analyzed, and the annual averages of cloud cover in the Arctic region were found to be 66.8%, 78.4%, and 63.3% as derived from MODIS, CALIOP, and CPR, respectively. A large disagreement between MODIS and CALIOP over sea ice and Greenland is observed, with a cloud percentage difference of 30.9% and 31.5%, respectively. In the entire Arctic, the average disagreement between MODIS and CALIOP increased from 13.1% during daytime to 26.7% during nighttime. Furthermore, the MODIS cloud mask accuracy has a high seasonal dependence, in that MODIS-CALIOP disagreement is the lowest during summertime at 10.7% and worst during winter at 28.0%. During nighttime the magnitude of the bias is higher because cloud detection is limited to the use of infrared bands. The clouds not detected by MODIS are typically low-level (top height <2 km) and high-level clouds (top height >6 km) and, especially, those that are geometrically thin (<2 km). Geometrically thin clouds (<2 km) accounted for about 95.5% of all clouds that CPR misses. As reported in a similar study, very low and thin clouds (<0.3 km) over sea ice that are detected by MODIS are sometimes not observed by CPR and misclassified by CALIOP. C1 [Chan, Mark Aaron; Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chan, Mark Aaron] De La Salle Univ, Ctr Engn & Sustainable Dev Res, Manila 1004, Philippines. RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM josefino.c.comiso@nasa.gov FU NASA Cryospheric Sciences program FX We thank the MODIS, CloudSat, CALIPSO, and AMSR-E science teams for providing excellent and accessible data products that made this study possible. These data were obtained from the National Snow and Ice Data Center (http://nsidc.org), the NASA Langley Research Center Atmospheric Science Data Center (http://eosweb.larc.nasa.gov/), the NASA LAADSWeb (http://ladsweb.nascom.nasa.gov/), and the CloudSat data processing center (http://cloudsat.cira.colostate.edu/). The NASA Cryospheric Sciences program in part funds this project. NR 26 TC 16 Z9 16 U1 2 U2 22 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 MAY PY 2013 VL 26 IS 10 BP 3285 EP 3306 DI 10.1175/JCLI-D-12-00204.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 142DG UT WOS:000318775900018 ER PT J AU Geogdzhayev, I Cairns, B Alexandrov, M Mishchenko, MI AF Geogdzhayev, Igor Cairns, Brian Alexandrov, Mikhail Mishchenko, Michael I. TI Statistical analysis of single-track instrument sampling in spaceborne aerosol remote sensing for climate research SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Tropospheric aerosols; Satellite remote sensing; Climate change; Aerosol climatology; Long-term variability ID UNIFIED SATELLITE CLIMATOLOGY; OPTICAL-PROPERTIES; MODIS; MISR; RETRIEVAL; AERONET; MISSION; LAND; REFLECTANCE; ABSORPTION AB We examine likely effects of pixel-wide along-track sampling on climatological means of aerosol optical thickness (AOT) derived from observations with satellite instruments such as CALIOP and APS by sub-sampling AOT retrievals from a wide-swath imaging instrument (MODIS). The advantage of using daily pixel-level aerosol retrievals from MODIS rather than aerosol transport models to assess the results of along-track sampling is that limitations caused by the presence of clouds are implicit in the satellite dataset, so that their seasonal and regional variations are captured coherently. However, imager data can exhibit latitudinal (cross-track) variability of monthly global mean AOTs caused by a scattering-angle dependence. This makes it difficult to separate natural variability from viewing-geometry artifacts complicating direct comparisons of an along-track sub-sample with the full imager data. To work around this problem, we introduce "latitudinal-track" sampling which, by design, captures the cross-track AOT variability of the original imager data. We show that the latitudinal-track standard error of global monthly mean AOTs is much smaller than the longitudinal-track one. This allows us to attribute the difference between the two errors to MODIS viewing-geometry artifacts and obtain an upper limit on AOT errors caused by along-track sampling. We conclude that single-track instruments provide AOT sampling sufficient for climate applications. Since AOT is believed to be the most variable characteristic of tropospheric aerosols, our results imply that pixel-wide along-track coverage also provides adequate statistical representation of the global distribution of aerosol microphysical parameters. cl (C) 2013 Elsevier Ltd. All rights reserved. C1 [Geogdzhayev, Igor; Alexandrov, Mikhail] Columbia Univ, New York, NY 10025 USA. [Geogdzhayev, Igor; Cairns, Brian; Alexandrov, Mikhail; Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Geogdzhayev, I (reprint author), Columbia Univ, 2880 Broadway, New York, NY 10025 USA. EM igor.v.geogdzhayev@nasa.gov RI Mishchenko, Michael/D-4426-2012; OI Cairns, Brian/0000-0002-1980-1022 FU research division of the NASA FX We thank Li Liu for help with MODIS level-2 data and two anonymous reviewers whose insightful comments resulted in a much improved manuscript. This study was supported by the research division of the NASA Glory Mission Project managed by Hal Maring. NR 38 TC 2 Z9 2 U1 0 U2 7 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 MAY PY 2013 VL 121 BP 69 EP 77 DI 10.1016/j.jqsrt.2013.02.003 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 136TO UT WOS:000318386500007 ER PT J AU Brandis, AM Johnston, CO Cruden, BA Prabhu, DK Wray, AA Liu, Y Schwenke, DW Bose, D AF Brandis, A. M. Johnston, C. O. Cruden, B. A. Prabhu, D. K. Wray, A. A. Liu, Y. Schwenke, D. W. Bose, D. TI Validation of CO 4th positive radiation for Mars entry SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE CO 4th positive; Radiation; Validation; Spectroscopic database; Shock tube; Mars ID LUNAR-RETURN CONDITIONS; SHOCK-LAYER RADIATION; DIATOMIC-MOLECULES; CO2-N-2 PLASMAS; BASIS-SETS AB This paper presents measurements and simulations of CO 4th Positive equilibrium radiation obtained in the NASA Ames Research Center's Electric Arc Shock Tube (EAST) facility. The experiments were aimed at measuring the level of radiation encountered during conditions relevant to high-speed entry into a simulated Martian atmosphere (96% CO2: 4% N-2). The facility was configured to target several ranges of nominal Mars entry conditions, of which 7.35 km/s at 0.1 Torr (13.3 Pa), 6.2-8 km/s at 0.25 Torr (33 Pa) and 7.1-7.8 km/s at 1 Torr (133 Pa) are examined in this paper. The CO 4th Positive system was chosen to be the focus of this study as it accounts for a large percentage of the emitted radiation for Martian entry, and also due to the difficulties of obtaining experimental validation data due to the emission appearing in the Vacuum Ultra Violet (VUV) spectral range. The focus of this paper is to provide a comprehensive comparison between the EAST data and various CO 4th Positive databases available in the literature. The analysis endeavors to provide a better understanding of the uncertainty in the measurements and quantifies the level of agreement found between simulations and experimental data. The results of the analysis show that the magnitude of the CO 4th Positive radiative intensity is very sensitive to the flow temperature. Subsequently, simulations using thermodynamic equilibrium generally under-predict the experimental data by approximately a factor of up to 2. However, when simulations are performed using a flow temperature extracted from the black body limited portion of the CO 4th Positive spectra taken from experiment, the agreement between the EAST data and simulations is generally very good. Furthermore, comparisons of experimental data and simulations across other spectral regions provide additional support for the use of the black body temperature. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Brandis, A. M.] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, Mountain View, CA 94035 USA. [Johnston, C. O.] NASA, Langley Res Ctr, Hampton, VA 23669 USA. [Brandis, A. M.; Cruden, B. A.; Prabhu, D. K.] ERC Corp, Mountain View, CA 94035 USA. [Wray, A. A.; Liu, Y.; Schwenke, D. W.; Bose, D.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Brandis, AM (reprint author), ERC Corp, Mountain View, CA 94035 USA. EM aaron.m.brandis@nasa.gov RI schwenke, david/I-3564-2013 NR 34 TC 6 Z9 6 U1 0 U2 5 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 MAY PY 2013 VL 121 BP 91 EP 104 DI 10.1016/j.jqsrt.2013.02.009 PG 14 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 136TO UT WOS:000318386500009 ER PT J AU Myint, SW Wentz, EA Brazel, AJ Quattrochi, DA AF Myint, Soe W. Wentz, Elizabeth A. Brazel, Anthony J. Quattrochi, Dale A. TI The impact of distinct anthropogenic and vegetation features on urban warming SO LANDSCAPE ECOLOGY LA English DT Article DE Land surface temperature; Urban land cover; QuickBird; ASTER; High albedo roof; Dark surface; Phoenix ID REMOTE-SENSING DATA; LAND-SURFACE TEMPERATURE; HEAT-ISLAND; METROPOLITAN REGION; PHOENIX; COVER; WATER; URBANIZATION; CLIMATES; LANDSCAPES AB We investigate the direct relationship between detailed urban land cover classes, derived from fine resolution QuickBird satellite data, and land surface temperatures (Celsius), generated from ASTER imagery, over Phoenix, Arizona. Using daytime and nighttime temperatures in both winter and summer and all observation points (n = 11,025), we develop linear, non-linear and multiple regression models to explore the relationship. Conventional wisdom suggests that all urban features result in increased temperatures. Rather, our results show that a mass of buildings is not necessarily or holistically responsible for extreme heat in desert cities. It is the construction of other impervious dark surfaces (i.e., asphalt roads) associated with buildings that result in extreme heat. Moreover, our results suggest that buildings, especially commercial buildings with high albedo roofs, actually reduce temperatures. The addition of trees and shrubs, as opposed to grass, around buildings can further mitigate extreme heat by providing more cooling during the summer and increasing nighttime temperatures in the winter. In conclusion, the compositional design of and avoidance of dark impervious materials in desert cities help mitigate extreme temperatures. It is important to note, however, that design choices that reduce extreme heat must be made within the broader context of tradeoffs and unintended consequences to ensure the sustainability of these cities. C1 [Myint, Soe W.; Wentz, Elizabeth A.; Brazel, Anthony J.] Arizona State Univ, Sch Geog Sci & Urban Planning, Tempe, AZ 85287 USA. [Quattrochi, Dale A.] NASA, Earth Sci Off, Marshall Spaceflight Ctr, Huntsville, AL 35812 USA. RP Myint, SW (reprint author), Arizona State Univ, Sch Geog Sci & Urban Planning, Coor Hall,5th Floor,975 S Myrtle Ave, Tempe, AZ 85287 USA. EM soe.myint@asu.edu FU National Science Foundation [SES-0951366] FX This research was supported by the National Science Foundation (Grant SES-0951366, Decision Center for a Desert City II: Urban Climate Adaptation). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the sponsoring agencies. NR 54 TC 27 Z9 28 U1 4 U2 70 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2973 J9 LANDSCAPE ECOL JI Landsc. Ecol. PD MAY PY 2013 VL 28 IS 5 BP 959 EP 978 DI 10.1007/s10980-013-9868-y PG 20 WC Ecology; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 138FO UT WOS:000318494500013 ER PT J AU Jones, JS Sharon, JA Mohammed, JS Hemker, KJ AF Jones, Justin S. Sharon, John A. Mohammed, Jelila S. Hemker, Kevin J. TI Small-scale mechanical characterization of space-exposed fluorinated ethylene propylene recovered from the Hubble Space Telescope SO POLYMER TESTING LA English DT Article DE Space-exposure; Small-scale tensile testing; Chain scission; Digital image correlation; Fluorinated ethylene propylene ID TEFLON(R) FEP; POLY(TETRAFLUOROETHYLENE-CO-HEXAFLUOROPROPYLENE); DEGRADATION; IRRADIATION; POLYMER AB Multi-layer insulation (MLI) blankets from the Hubble Space Telescope have been recovered during the last servicing mission, after 19.1 years of on-orbit service. Based on testing and analysis of returned insulation material from earlier Hubble servicing missions, the space environment is known to have detrimental effects on the mechanical properties. The most recently retrieved MLI blankets were highly degraded with many cracks, limiting the material available for full-scale mechanical testing. As a result, micro-tensile experiments have been performed to characterize the effect of space exposure on the mechanical response of the outermost layer of the MLI This outer layer, 127 mu m thick fluorinated ethylene propylene with a 100 nm thick vapor deposited aluminum reflective coating, maintained significant tensile ductility but exhibited a degradation of strength that scales with severity of space exposure. This change in properties is attributed to damage from incident solar flux, atomic oxygen damage and thermal cycling. Published by Elsevier Ltd. C1 [Jones, Justin S.; Mohammed, Jelila S.] NASA, Mat Engn Branch Code 541, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sharon, John A.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Hemker, Kevin J.] Johns Hopkins Univ, Dept Mech Engn, Baltimore, MD 21218 USA. RP Jones, JS (reprint author), NASA, Mat Engn Branch Code 541, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM justin.s.jones@nasa.gov; jasharo@sandia.gov; jelila.s.mohammed@nasa.gov; hemker@jhu.edu NR 18 TC 0 Z9 0 U1 3 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0142-9418 J9 POLYM TEST JI Polym. Test PD MAY PY 2013 VL 32 IS 3 BP 602 EP 607 DI 10.1016/j.polymertesting.2013.02.004 PG 6 WC Materials Science, Characterization & Testing; Polymer Science SC Materials Science; Polymer Science GA 136RQ UT WOS:000318381500020 ER PT J AU Granat, R Parker, J Kedar, S Dong, DA Tang, BY Bock, Y AF Granat, Robert Parker, Jay Kedar, Sharon Dong, Danan Tang, Benyang Bock, Yehuda TI Statistical Approaches to Detecting Transient Signals in GPS: Results from the 2009-2011 Transient Detection Exercise SO SEISMOLOGICAL RESEARCH LETTERS LA English DT Article ID HIDDEN MARKOV-MODELS; CONTINUOUS SPEECH RECOGNITION; CASCADIA SUBDUCTION ZONE; NORTHRIDGE EARTHQUAKE; CRUSTAL DEFORMATION; HECTOR MINE; SLIP; SILENT; SLOW; ALGORITHM C1 [Granat, Robert; Parker, Jay; Kedar, Sharon; Tang, Benyang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dong, Danan] E China Normal Univ, Shanghai 200062, Peoples R China. [Bock, Yehuda] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Granat, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.a.granat@jpl.nasa.gov FU NASA's Advanced Information Systems Technology (AIST) program; Southern California Earthquake Center (SCEC) FX This research was carried out at the Jet Propulsion Laboratory GM California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Funding for this work was provided by NASA's Advanced Information Systems Technology (AIST) program and by the Southern California Earthquake Center (SCEC). NR 46 TC 5 Z9 5 U1 0 U2 2 PU SEISMOLOGICAL SOC AMER PI ALBANY PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA SN 0895-0695 EI 1938-2057 J9 SEISMOL RES LETT JI Seismol. Res. Lett. PD MAY-JUN PY 2013 VL 84 IS 3 BP 444 EP 454 DI 10.1785/0220130039 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 135ZA UT WOS:000318328000005 ER PT J AU Campbell, JF AF Campbell, Joel F. TI Nonlinear swept frequency technique for CO2 measurements using a CW laser system SO APPLIED OPTICS LA English DT Article ID ABSORPTION; MODULATION; DESIGN; SIGNAL; LIDAR AB A system using a nonlinear multiswept sine wave is described, which employs multichannel multiswept orthogonal waves, to separate channels and make multiple, simultaneous online/offline CO2 measurements. An analytic expression and systematic method for determining the orthogonal frequencies for the unswept, linear swept, and nonlinear swept cases is presented. It is shown that one may reduce sidelobes of the autocorrelation function while preserving cross channel orthogonality, for thin cloud rejection. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Campbell, JF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM joel.f.campbell@nasa.gov NR 24 TC 7 Z9 7 U1 0 U2 4 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X J9 APPL OPTICS JI Appl. Optics PD MAY 1 PY 2013 VL 52 IS 13 BP 3100 EP 3107 DI 10.1364/AO.52.003100 PG 8 WC Optics SC Optics GA 137FW UT WOS:000318421900021 PM 23669780 ER PT J AU Bhat, NDR Chengalur, JN Cox, PJ Gupta, Y Prasad, J Roy, J Bailes, M Burke-Spolaor, S Kudale, SS van Straten, W AF Bhat, N. D. R. Chengalur, J. N. Cox, P. J. Gupta, Y. Prasad, J. Roy, J. Bailes, M. Burke-Spolaor, S. Kudale, S. S. van Straten, W. TI DETECTION OF FAST TRANSIENTS WITH RADIO INTERFEROMETRIC ARRAYS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE instrumentation: interferometers; methods: observational; pulsars: individual (J1752-2806); techniques: interferometric ID REFRACTIVE INTERSTELLAR SCINTILLATION; UNIVERSE PULSAR SURVEY; MULTIFREQUENCY OBSERVATIONS; GIANT PULSES; REAL-TIME; SEARCHES; TELESCOPE; EMISSION; MAGNETAR; BURSTS AB Next-generation radio arrays, including the Square Kilometre Array (SKA) and its pathfinders, will open up new avenues for exciting transient science at radio wavelengths. Their innovative designs, comprising a large number of small elements, pose several challenges in digital processing and optimal observing strategies. The Giant Metre-wave Radio Telescope (GMRT) presents an excellent test-bed for developing and validating suitable observing modes and strategies for transient experiments with future arrays. Here we describe the first phase of the ongoing development of a transient detection system for GMRT that is planned to eventually function in a commensal mode with other observing programs. It capitalizes on the GMRT's interferometric and sub-array capabilities, and the versatility of a new software backend. We outline considerations in the plan and design of transient exploration programs with interferometric arrays, and describe a pilot survey that was undertaken to aid in the development of algorithms and associated analysis software. This survey was conducted at 325 and 610 MHz, and covered 360 deg(2) of the sky with short dwell times. It provides large volumes of real data that can be used to test the efficacies of various algorithms and observing strategies applicable for transient detection. We present examples that illustrate the methodologies of detecting short-duration transients, including the use of sub-arrays for higher resilience to spurious events of terrestrial origin, localization of candidate events via imaging, and the use of a phased array for improved signal detection and confirmation. In addition to demonstrating applications of interferometric arrays for fast transient exploration, our efforts mark important steps in the roadmap toward SKA-era science. C1 [Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Bhat, N. D. R.; Cox, P. J.; Bailes, M.; Burke-Spolaor, S.; van Straten, W.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bhat, N. D. R.; Bailes, M.; van Straten, W.] Curtin Univ, Australian Res Council, Ctr Excellence All Sky Astrophys CAASTRO, Bentley, WA 6102, Australia. [Chengalur, J. N.; Gupta, Y.; Roy, J.; Kudale, S. S.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Cox, P. J.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Prasad, J.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Burke-Spolaor, S.] NASA, Jet Prop Lab, Pasadena, CA 91106 USA. RP Bhat, NDR (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. OI Cox, Peter/0000-0002-6157-3430; van Straten, Willem/0000-0003-2519-7375 FU Australian Government under the Australia-India Strategic Research Fund [ST020071]; Indian Government under the Department of Science and Technology [DST/INT/AUS/Proj-14/2008]; Curtin Research Fellowship; [CE11E0090] FX This work is supported by the Australian Government under the Australia-India Strategic Research Fund grant ST020071 and by the Indian Government under the Department of Science and Technology grant DST/INT/AUS/Proj-14/2008. The Centre for All-sky Astrophysics is an Australian Research Council Centre for Excellence, funded by CE11E0090. N.D.R.B. is supported by a Curtin Research Fellowship and thanks Steven Tingay for support and encouragement extended to this project. We thank an anonymous referee for many useful comments that helped to improve the clarity of the paper. Data processing was carried out at Swinburne University's Supercomputing Facility. We thank the staff of the GMRT for help with the observations. The GMRT is operated by the National Centre for Radio Astrophysics (NCRA) of the Tata Institute of Fundamental Research (TIFR), India. NR 53 TC 5 Z9 5 U1 0 U2 5 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 MAY PY 2013 VL 206 IS 1 AR 2 DI 10.1088/0067-0049/206/1/2 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139BK UT WOS:000318556300002 ER PT J AU Scoville, N Arnouts, S Aussel, H Benson, A Bongiorno, A Bundy, K Calvo, MAA Capak, P Carollo, M Civano, F Dunlop, J Elvis, M Faisst, A Finoguenov, A Fu, H Giavalisco, M Guo, Q Ilbert, O Iovino, A Kajisawa, M Kartaltepe, J Leauthaud, A Le Fevre, O LeFloch, E Lilly, SJ Liu, CTC Manohar, S Massey, R Masters, D McCracken, HJ Mobasher, B Peng, YJ Renzini, A Rhodes, J Salvato, M Sanders, DB Sarvestani, BD Scarlata, C Schinnerer, E Sheth, K Shopbell, PL Smolcic, V Taniguchi, Y Taylor, JE White, SDM Yan, L AF Scoville, N. Arnouts, S. Aussel, H. Benson, A. Bongiorno, A. Bundy, K. Calvo, M. A. A. Capak, P. Carollo, M. Civano, F. Dunlop, J. Elvis, M. Faisst, A. Finoguenov, A. Fu, Hai Giavalisco, M. Guo, Q. Ilbert, O. Iovino, A. Kajisawa, M. Kartaltepe, J. Leauthaud, A. Le Fevre, O. LeFloch, E. Lilly, S. J. Liu, C. T. -C. Manohar, S. Massey, R. Masters, D. McCracken, H. J. Mobasher, B. Peng, Y. -J. Renzini, A. Rhodes, J. Salvato, M. Sanders, D. B. Sarvestani, B. D. Scarlata, C. Schinnerer, E. Sheth, K. Shopbell, P. L. Smolcic, V. Taniguchi, Y. Taylor, J. E. White, S. D. M. Yan, L. TI EVOLUTION OF GALAXIES AND THEIR ENVIRONMENTS AT z=0.1-3 IN COSMOS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: evolution; large-scale structure of universe ID VLT DEEP SURVEY; STAR-FORMATION HISTORY; SIMILAR-TO 1.4; REDSHIFT SURVEY; STELLAR MASS; PHOTOMETRIC REDSHIFTS; FORMING GALAXIES; DENSITY RELATION; CLUSTER SURVEY; LEGACY SURVEY AB Large-scale structures (LSSs) out to z < 3.0 are measured in the Cosmic Evolution Survey (COSMOS) using extremely accurate photometric redshifts (photoz). The K-s-band-selected sample (from Ultra-Vista) is comprised of 155,954 galaxies. Two techniques-adaptive smoothing and Voronoi tessellation-are used to estimate the environmental densities within 127 redshift slices. Approximately 250 statistically significant overdense structures are identified out to z = 3.0 with shapes varying from elongated filamentary structures to more circularly symmetric concentrations. We also compare the densities derived for COSMOS with those based on semi-analytic predictions for Lambda CDM simulation and find excellent overall agreement between the mean densities as a function of redshift and the range of densities. The galaxy properties (stellar mass, spectral energy distributions (SEDs), and star formation rates (SFRs)) are strongly correlated with environmental density and redshift, particularly at z < 1.0-1.2. Classifying the spectral type of each galaxy using the rest-frame b - i color (from the photoz SED fitting), we find a strong correlation of early-type galaxies (E-Sa) with high-density environments, while the degree of environmental segregation varies systematically with redshift out to z similar to 1.3. In the highest density regions, 80% of the galaxies are early types at z = 0.2 compared to only 20% at z = 1.5. The SFRs and the star formation timescales exhibit clear environmental correlations. At z > 0.8, the SFR density is uniformly distributed over all environmental density percentiles, while at lower redshifts the dominant contribution is shifted to galaxies in lower density environments. C1 [Scoville, N.; Benson, A.; Fu, Hai; Manohar, S.; Rhodes, J.; Salvato, M.; Shopbell, P. L.; Smolcic, V.] CALTECH, Pasadena, CA 91125 USA. [Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Arnouts, S.; Kartaltepe, J.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Aussel, H.; LeFloch, E.] Univ Paris 07, CNRS, AIM Unite Mixte Rech CEA, UMR 158, Paris, France. [Benson, A.] Carnegie Observ, Pasadena, CA USA. [Bongiorno, A.] Osserv Astron Roma, INAF, I-00040 Pomezia, Italy. [Bundy, K.; Leauthaud, A.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778582, Japan. [Calvo, M. A. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Capak, P.; Yan, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Carollo, M.; Faisst, A.; Lilly, S. J.; Peng, Y. -J.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunlop, J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Finoguenov, A.; Guo, Q.; Salvato, M.; White, S. D. M.] Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. [Fu, Hai] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA. [Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Guo, Q.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Ilbert, O.; Le Fevre, O.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Iovino, A.] Osserv Astron Brera, INAF, I-20159 Milan, Italy. [Kajisawa, M.; Taniguchi, Y.] Ehime Univ, Grad Sch Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Liu, C. T. -C.] CUNY Coll Staten Isl, Dept Engn Sci & Phys, Astrophys Observ, Staten Isl, NY 10314 USA. [Liu, C. T. -C.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Liu, C. T. -C.] Amer Museum Nat Hist, Hayden Planetarium, New York, NY 10024 USA. [Massey, R.] Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Masters, D.; Mobasher, B.; Sarvestani, B. D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [McCracken, H. J.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Renzini, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Scarlata, C.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Sheth, K.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Smolcic, V.] Argelander Inst Astron, D-53121 Bonn, Germany. [Taylor, J. E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. RP Scoville, N (reprint author), CALTECH, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. OI Iovino, Angela/0000-0001-6958-0304; Bongiorno, Angela/0000-0002-0101-6624; Schinnerer, Eva/0000-0002-3933-7677 FU NASA [12712786]; National Radio Astronomy Observatory; National basic research program of China (program 973) [2009CB24901]; Young Researcher Grant of National Astronomical Observatories, CAS; NSFC [11143005]; Partner Group program of the Max Planck Society FX We thank the referee for helpful suggestions that have very much improved this work and we thank Zara Scoville for proof-reading of the manuscript. Support for this work was provided by NASA through Contract Number 12712786 issued by JPL. Additional information on the COSMOS survey is available from the main COSMOS Web site at http://www.astro.caltech.edu/cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff in providing online archive and server capabilities for the COSMOS data sets. The environmental densities and mpeg versions with all 127 redshift slices of the maps shown in Figures 6-8 will be available in FITS format from the NASA IPAC/IRSA archive at http://irsa.ipac.caltech.edu/data/COSMOS/. K.S. acknowledges support from the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. G.Q. acknowledges support from the National basic research program of China (program 973 under grant No. 2009CB24901), the Young Researcher Grant of National Astronomical Observatories, CAS, the NSFC grants program (No. 11143005), and the Partner Group program of the Max Planck Society. NR 70 TC 61 Z9 61 U1 1 U2 5 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 MAY PY 2013 VL 206 IS 1 AR 3 DI 10.1088/0067-0049/206/1/3 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139BK UT WOS:000318556300003 ER PT J AU Stierwalt, S Armus, L Surace, JA Inami, H Petric, AO Diaz-Santos, T Haan, S Charmandaris, V Howell, J Kim, DC Marshall, J Mazzarella, JM Spoon, HWW Veilleux, S Evans, A Sanders, DB Appleton, P Bothun, G Bridge, CR Chan, B Frayer, D Iwasawa, K Kewley, LJ Lord, S Madore, BF Melbourne, JE Murphy, EJ Rich, JA Schulz, B Sturm, E U, V Vavilkin, T Xu, K AF Stierwalt, S. Armus, L. Surace, J. A. Inami, H. Petric, A. O. Diaz-Santos, T. Haan, S. Charmandaris, V. Howell, J. Kim, D. C. Marshall, J. Mazzarella, J. M. Spoon, H. W. W. Veilleux, S. Evans, A. Sanders, D. B. Appleton, P. Bothun, G. Bridge, C. R. Chan, B. Frayer, D. Iwasawa, K. Kewley, L. J. Lord, S. Madore, B. F. Melbourne, J. E. Murphy, E. J. Rich, J. A. Schulz, B. Sturm, E. U, V. Vavilkin, T. Xu, K. TI MID-INFRARED PROPERTIES OF NEARBY LUMINOUS INFRARED GALAXIES. I. SPITZER INFRARED SPECTROGRAPH SPECTRA FOR THE GOALS SAMPLE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: interactions; galaxies: nuclei; galaxies: starburst; infrared: galaxies ID POLYCYCLIC AROMATIC-HYDROCARBONS; SKY LIRG SURVEY; STAR-FORMATION; SPACE-TELESCOPE; SUBMILLIMETER GALAXIES; STARBURST GALAXIES; SPATIAL EXTENT; EMISSION; CONTINUUM; DUST AB The Great Observatories All-Sky LIRG Survey (GOALS) is a comprehensive, multiwavelength study of luminous infrared galaxies (LIRGs) in the local universe. Here we present low resolution Spitzer Infrared Spectrograph spectra covering 5-38 mu m and provide a basic analysis of the mid-IR spectral properties observed for nearby LIRGs. In a companion paper, we discuss detailed fits to the spectra and compare the LIRGs to other classes of galaxies. The GOALS sample of 244 nuclei in 180 luminous (10(11) <= L-IR/L-circle dot < 10(12)) and 22 ultraluminous (L-IR/L-circle dot >= 10(12)) IR galaxies represents a complete subset of the IRAS Revised Bright Galaxy Sample and covers a range of merger stages, morphologies, and spectral types. The majority (>60%) of the GOALS LIRGs have high 6.2 mu m polycyclic aromatic hydrocarbon (PAH) equivalent widths (EQW(6.2 mu m) > 0.4 mu m) and low levels of silicate absorption (s(9.7 mu m) > -1.0). There is a general trend among the U/LIRGs for both silicate depth and mid-infrared (MIR) slope to increase with increasing L-IR. U/LIRGs in the late to final stages of a merger also have, on average, steeper MIR slopes and higher levels of dust obscuration. Together, these trends suggest that as gas and dust is funneled toward the center of a coalescing merger, the nuclei become more compact and more obscured. As a result, the dust temperature increases also leading to a steeper MIR slope. The sources that depart from these correlations have very low PAH equivalent width (EQW(6.2 mu m) < 0.1 mu m) consistent with their emission being dominated by an active galactic nucleus (AGN) in the MIR. These extremely low PAH EQW sources separate into two distinct types: relatively unobscured sources with a very hot dust component (and thus very shallow MIR slopes) and heavily dust obscured nuclei with a steep temperature gradient. The most heavily dust obscured sources are also the most compact in their MIR emission, suggesting that the obscuring (cool) dust is associated with the outer regions of the starburst and not simply a measure of the dust along the line of sight through a large, dusty disk. A marked decline is seen for the fraction of high EQW (star formation dominated) sources as the merger progresses. The decline is accompanied by an increase in the fraction of composite sources while the fraction of sources where an AGN dominates the MIR emission remains low. When compared to the MIR spectra of submillimeter galaxies (SMGs) at z similar to 2, both the average GOALS LIRG and ULIRG spectra are more absorbed at 9.7 mu m and the average GOALS LIRG has more PAH emission. However, when the AGN contributions to both the local GOALS LIRGs and the high-z SMGs are removed, the average local starbursting LIRG closely resembles the starburst-dominated SMGs. C1 [Stierwalt, S.; Armus, L.; Surace, J. A.; Inami, H.; Petric, A. O.; Diaz-Santos, T.; Haan, S.; Howell, J.; Marshall, J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Stierwalt, S.; Evans, A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Inami, H.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Petric, A. O.; Bridge, C. R.; Melbourne, J. E.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Haan, S.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Charmandaris, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Charmandaris, V.] Univ Crete, ITCP, GR-71003 Iraklion, Greece. [Charmandaris, V.] Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece. [Charmandaris, V.] Observ Paris, F-75014 Paris, France. [Kim, D. C.; Evans, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Mazzarella, J. M.; Chan, B.; Lord, S.; Xu, K.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Spoon, H. W. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Sanders, D. B.; Kewley, L. J.; Rich, J. A.; U, V.] Univ Hawaii, Inst Astron, Honolulu, HI 96825 USA. [Appleton, P.; Schulz, B.] NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Bothun, G.] Univ Oregon, Dept Phys, Eugene, OR 97402 USA. [Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Iwasawa, K.] INAF Observ Astron Bologna, Bologna, Italy. [Madore, B. F.; Murphy, E. J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Sturm, E.] MPE, D-85741 Garching, Germany. [Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. RP Stierwalt, S (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM sabrinas@virginia.edu RI Charmandaris, Vassilis/A-7196-2008; OI Charmandaris, Vassilis/0000-0002-2688-1956; Rich, Jeffrey/0000-0002-5807-5078; Mazzarella, Joseph/0000-0002-8204-8619; Appleton, Philip/0000-0002-7607-8766 FU NASA [1407]; National Aeronautics and Space Administration FX The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics Space Administration. We thank M. Cluver for many helpful discussions and K. Menendez-Delmestre for sharing her average SMG spectra. NR 38 TC 49 Z9 49 U1 1 U2 7 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 MAY PY 2013 VL 206 IS 1 AR 1 DI 10.1088/0067-0049/206/1/1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139BK UT WOS:000318556300001 ER PT J AU Tenenbaum, P Jenkins, JM Seader, S Burke, CJ Christiansen, JL Rowe, JF Caldwell, DA Clarke, BD Li, J Quintana, EV Smith, JC Thompson, SE Twicken, JD Borucki, WJ Batalha, NM Cote, MT Haas, MR Hunter, RC Sanderfer, DT Girouard, FR Hall, JR Ibrahim, K Klaus, TC McCauliff, SD Middour, CK Sabale, A Uddin, AK Wohler, B Barclay, T Still, M AF Tenenbaum, Peter Jenkins, Jon M. Seader, Shawn Burke, Christopher J. Christiansen, Jessie L. Rowe, Jason F. Caldwell, Douglas A. Clarke, Bruce D. Li, Jie Quintana, Elisa V. Smith, Jeffrey C. Thompson, Susan E. Twicken, Joseph D. Borucki, William J. Batalha, Natalie M. Cote, Miles T. Haas, Michael R. Hunter, Roger C. Sanderfer, Dwight T. Girouard, Forrest R. Hall, Jennifer R. Ibrahim, Khadeejah Klaus, Todd C. McCauliff, Sean D. Middour, Christopher K. Sabale, Anima Uddin, Akm K. Wohler, Bill Barclay, Thomas Still, Martin TI DETECTION OF POTENTIAL TRANSIT SIGNALS IN THE FIRST 12 QUARTERS OF KEPLER MISSION DATA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; planets and satellites: detection AB We present the results of a search for potential transit signals in the first three years of photometry data acquired by the Kepler mission. The targets of the search include 112,321 targets that were observed over the full interval and an additional 79,992 targets that were observed for a subset of the full interval. From this set of targets we find a total of 11,087 targets that contain at least one signal that meets the Kepler detection criteria: periodicity of the signal, an acceptable signal-to-noise ratio, and three tests that reject false positives. Each target containing at least one detected signal is then searched repeatedly for additional signals, which represent multi-planet systems of transiting planets. When targets with multiple detections are considered, a total of 18,406 potential transiting planet signals are found in the Kepler mission data set. The detected signals are dominated by events with relatively low signal-to-noise ratios and by events with relatively short periods. The distribution of estimated transit depths appears to peak in the range between 20 and 30 parts per million, with a few detections down to fewer than 10 parts per million. The detections exhibit signal-to-noise ratios from 7.1 sigma, which is the lower cutoff for detections, to over 10,000 sigma, and periods ranging from 0.5 days, which is the shortest period searched, to 525 days, which is the upper limit of achievable periods given the length of the data set and the requirement that all detections include at least three transits. The detected signals are compared to a set of known transit events in the Kepler field of view, many of which were identified by alternative methods; the comparison shows that the current search recovery rate for targets with known transit events is 98.3%. C1 [Tenenbaum, Peter; Jenkins, Jon M.; Seader, Shawn; Burke, Christopher J.; Christiansen, Jessie L.; Rowe, Jason F.; Caldwell, Douglas A.; Clarke, Bruce D.; Li, Jie; Quintana, Elisa V.; Smith, Jeffrey C.; Thompson, Susan E.; Twicken, Joseph D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94305 USA. [Borucki, William J.; Batalha, Natalie M.; Cote, Miles T.; Haas, Michael R.; Hunter, Roger C.; Sanderfer, Dwight T.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. [Girouard, Forrest R.; Hall, Jennifer R.; Ibrahim, Khadeejah; Klaus, Todd C.; McCauliff, Sean D.; Middour, Christopher K.; Sabale, Anima; Uddin, Akm K.; Wohler, Bill] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94305 USA. [Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, BAER Inst, Moffett Field, CA 94305 USA. RP Tenenbaum, P (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94305 USA. EM peter.tenenbaum@nasa.gov RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU NASA's Space Mission Directorate FX Funding for this mission is provided by NASA's Space Mission Directorate. The contributions of Hema Chandrasekaran and Chris Henze have been essential in the studies documented here. NR 14 TC 34 Z9 34 U1 0 U2 5 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 MAY PY 2013 VL 206 IS 1 AR 5 DI 10.1088/0067-0049/206/1/5 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139BK UT WOS:000318556300005 ER PT J AU Halbig, MC Coddington, BP Asthana, R Singh, M AF Halbig, M. C. Coddington, B. P. Asthana, R. Singh, M. TI Characterization of silicon carbide joints fabricated using SiC particulate-reinforced Ag-Cu-Ti alloys SO CERAMICS INTERNATIONAL LA English DT Article DE Silicon carbide; Brazing; Particulate; Microhardness ID BRAZING ALLOY; COMPOSITE; CERAMICS; STRESSES AB CVD silicon carbide was brazed to itself using two Ag-Cu-Ti braze alloys reinforced with SiC particulates to control braze thermal expansion and enhance joint strength. Powders of the braze alloys, Ticusil (composition in wt%: Ag-26.7Cu-4.5Ti, T-L: 900 degrees C) and Cusil-ABA (Ag-35.3Cu-1.75Ti, T-L: 815 degrees C) were pre-mixed with 5, 10 and 15 wt% SiC particulates (similar to 20-30 mu m) using glycerin to create braze pastes that were applied to the surfaces to be joined. Joints were vacuum brazed and examined using optical microscopy (OM), field emission scanning electron microscopy (FESEM), energy dispersive spectroscopy (EDS) and the Knoop hardness test. The SiC particles were randomly distributed in the braze matrix and bonded to it via reaction with the titanium from the braze alloy. Titanium together with Si and C segregated at the particle/braze interface, and promoted nucleation and precipitation of the Cu-rich secondary phase on particle surfaces. The Si-Ti-C-rich reaction layers also formed at the interface between CVD SiC substrate and the braze alloy. The loss of Ti in the reaction with SiC particulates did not impair either the bond quality or the thickness of the reaction layer on the CVD SiC substrate. Microhardness measurements showed that the dispersed SiC particulates lowered the braze hardness by depleting the braze matrix of Ti. Theoretical calculations indicated the CTE of the braze to decrease by nearly 45-60% with the incorporation of about 45 vol% SiC. (C) 2012 Elsevier Ltd and Techna Group S.r.l. All rights reserved. C1 [Halbig, M. C.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Coddington, B. P.] Univ Wisconsin, Madison, WI USA. [Asthana, R.] Univ Wisconsin Stout, Menomonie, WI USA. [Singh, M.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH USA. RP Asthana, R (reprint author), Univ Wisconsin Stout, Menomonie, WI USA. EM AsthanaR@uwstout.edu FU NASA Glenn Research Center, Cleveland, OH FX B.P. Coddington and R. Asthana acknowledge the research support received from the NASA Glenn Research Center, Cleveland, OH. NR 28 TC 23 Z9 24 U1 3 U2 62 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0272-8842 J9 CERAM INT JI Ceram. Int. PD MAY PY 2013 VL 39 IS 4 BP 4151 EP 4162 DI 10.1016/j.ceramint.2012.10.271 PG 12 WC Materials Science, Ceramics SC Materials Science GA 133HI UT WOS:000318129100088 ER PT J AU Farnocchia, D Chesley, SR Vokrouhlicky, D Milani, A Spoto, F Bottke, WF AF Farnocchia, D. Chesley, S. R. Vokrouhlicky, D. Milani, A. Spoto, F. Bottke, W. F. TI Near Earth Asteroids with measurable Yarkovsky effect SO ICARUS LA English DT Article DE Asteroids, Dynamics; Celestial mechanics; Near-Earth objects; Orbit determination ID MAGNITUDE; FRAGMENTS; GOLEVKA; DRIFTS; MASSES; MODEL AB We seek evidence of the Yarkovsky effect among Near Earth Asteroids (NEAs) by measuring the Yarkovsky-related orbital drift from the orbital fit. To prevent the occurrence of unreliable detections we employ a high precision dynamical model, including the Newtonian attraction of 16 massive asteroids and the planetary relativistic terms, and a suitable astrometric data treatment. We find 21 NEAs whose orbital fits show a measurable orbital drift with a signal to noise ratio (SNR) greater than 3. The best determination is for asteroid (101955) 1999 RQ(36), with an SNR similar to 200. In some cases it is possible to constrain physical quantities otherwise unknown. Furthermore, the distribution of the detected orbital drifts shows an excess of retrograde rotators that can be connected to the delivery mechanism from the most important NEA feeding resonances and allows us to infer the obliquity distribution of NEAs. We discuss the implications of the Yarkovsky effect for impact predictions. In particular, for asteroid (29075) 1950 DA our results favor a retrograde rotation, which may have implications for the 2880 impact threat. (C) 2013 Elsevier Inc. All rights reserved. C1 [Farnocchia, D.; Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Farnocchia, D.] SpaceDyS, I-56023 Pisa, Italy. [Vokrouhlicky, D.] Charles Univ Prague, Inst Astron, CZ-18000 Prague 8, Czech Republic. [Milani, A.; Spoto, F.] Univ Pisa, Dept Math, I-56127 Pisa, Italy. [Bottke, W. F.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. RP Farnocchia, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Davide.Farnocchia@jpl.nasa.gov FU Czech Grant Agency [205/08/0064]; Czech Ministry of Education [MSM002162 0860]; NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology; NASA; ESA/ESTEC-SpaceDyS Service [SSA-NEO-ESA-SLA2-002_NEODYS] FX D.F. was supported for this research in part by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA, and in part by ESA/ESTEC-SpaceDyS Service Level Agreement SSA-NEO-ESA-SLA2-002_NEODYS.; The work of D.V. was partially supported by the Czech Grant Agency (Grant 205/08/0064) and Research Program MSM002162 0860 of the Czech Ministry of Education. NR 48 TC 32 Z9 32 U1 0 U2 9 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 MAY PY 2013 VL 224 IS 1 BP 1 EP 13 DI 10.1016/j.icarus.2013.02.004 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133HC UT WOS:000318128500001 ER PT J AU Konovalenko, AA Kalinichenko, NN Rucker, HO Lecacheux, A Fischer, G Zarka, P Zakharenko, VV Mylostna, KY Griessmeier, JM Abranin, EP Falkovich, IS Sidorchuk, KM Kurth, WS Kaiser, ML Gurnett, DA AF Konovalenko, A. A. Kalinichenko, N. N. Rucker, H. O. Lecacheux, A. Fischer, G. Zarka, P. Zakharenko, V. V. Mylostna, K. Y. Griessmeier, J. -M. Abranin, E. P. Falkovich, I. S. Sidorchuk, K. M. Kurth, W. S. Kaiser, M. L. Gurnett, D. A. TI Earliest recorded ground-based decameter wavelength observations of Saturn's lightning during the giant E-storm detected by Cassini spacecraft in early 2006 SO ICARUS LA English DT Article DE Saturn; Lightning; Radio observations; Saturn, Atmosphere ID RED SPRITES; PULSE PAIRS; RADIO; SYSTEM; THUNDERSTORM; DISCHARGES; BURSTS; MHZ AB We report the history of the first recorded ground-based radio detection of Saturn's lightning using the Ukrainian UTR-2 radiotelescope at frequencies from 20 to 25 MHz. The observations were performed between 29 January and 3 February 2006, during which lighting activity (E-storm) on Saturn was detected by the radio experiment onboard Cassini spacecraft. The minimum detectable flux density (1 sigma-level) at UTR-2 reached 40 Jy (1 Jy = 10(-26) Wm(-2) Hz(-1)) for narrowband observations (Delta f = 10 kHz) and 4 Jy for broadband observations (Delta f = 1 MHz), for an effective telescope area of approximate to 100,000 m(2) and integration time of 20 ms. Selection criteria including comparison of simultaneous ON/OFF-source observations were applied to distinguish detection of lightning-associated radio pulses from interference. This allowed us to identify about 70 events with signal-to-noise ratio more than 5. Measured flux densities (between 50 and 700 Jy) and burst durations (between 60 and 220 ms) are in good agreement with extrapolation of previous Cassini measurements to a ground-based observer. This first detection demonstrates the possibility of Solar System planetary lightning studies using large, present and future ground-based radio instruments. The developed methods of observations and identification criteria are also implemented on the UTR-2 radio telescope for the investigation of the next Saturn's storms. Together with recently published UTR-2 measurements of activity measured after the 2006 storm reported here, the results have significant implications for detectable planetary radio emission in our Solar System and beyond. (C) 2012 Elsevier Inc. All rights reserved. C1 [Konovalenko, A. A.; Kalinichenko, N. N.; Zakharenko, V. V.; Mylostna, K. Y.; Abranin, E. P.; Falkovich, I. S.; Sidorchuk, K. M.] Inst Radio Astron, UA-61002 Kharkov, Ukraine. [Rucker, H. O.; Fischer, G.] Space Res Inst, A-8042 Graz, Austria. [Lecacheux, A.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [Zarka, P.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France. [Griessmeier, J. -M.] LPC2E, F-45071 Orleans 2, France. [Kurth, W. S.; Gurnett, D. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Konovalenko, AA (reprint author), Inst Radio Astron, 4 Chervonopraporna Str, UA-61002 Kharkov, Ukraine. EM akonov@ri.kharkov.ua OI Kurth, William/0000-0002-5471-6202 FU ANR [NT05-1 42530]; NASU-CNRS PICS Program [1.33.11]; Ukrainian State Fund for Fundamental Researches [F28.2/005]; CNES (Centre National d'Etudes Spatiales); National Academy of Sciences of Ukraine; Russian Foundation for Basic Research FX This work was initiated and partly supported by ANR Program NT05-1 42530 "Radio-Exopla", and pursued in the frame of the NASU-CNRS PICS Program "Development of LF radioastronomy with ultrahigh sensitivity and resolution" (Grant 1.33.11). This work is also partially supported by the Ukrainian State Fund for Fundamental Researches (Project F28.2/005). Cassini activities in LESIA are supported by the CNES (Centre National d'Etudes Spatiales). This work is also supported by the National Academy of Sciences of Ukraine and the Russian Foundation for Basic Research (Ukrainian-Russian Project 2012). We thank both the referees for the very useful comments. NR 33 TC 6 Z9 6 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2013 VL 224 IS 1 BP 14 EP 23 DI 10.1016/j.icarus.2012.07.024 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133HC UT WOS:000318128500002 ER PT J AU Moskovitz, NA Abe, S Pan, KS Osip, DJ Pefkou, D Melita, MD Elias, M Kitazato, K Bus, SJ DeMeo, FE Binzel, RP Abell, PA AF Moskovitz, Nicholas A. Abe, Shinsuke Pan, Kang-Shian Osip, David J. Pefkou, Dimitra Melita, Mario D. Elias, Mauro Kitazato, Kohei Bus, Schelte J. DeMeo, Francesca E. Binzel, Richard P. Abell, Paul A. TI Rotational characterization of Hayabusa II target Asteroid (162173) 1999 JU3 SO ICARUS LA English DT Article DE Asteroids; Asteroids, Rotation; Asteroids, Composition; Photometry; Spectroscopy ID NEAR-EARTH ASTEROIDS; CARBONACEOUS CHONDRITES; THERMAL METAMORPHISM; 4 VESTA; ITOKAWA; ALBEDO; PHASE; HETEROGENEITY; SPECTROSCOPY; METEORITES AB The Japanese Space Agency's Hayabusa II mission is scheduled to rendezvous with and return a sample from the near-Earth Asteroid (162173) 1999 JU3. Previous visible-wavelength spectra of this object show significant variability across multiple epochs which has been attributed to a compositionally heterogeneous surface. We present new visible and near-infrared spectra to demonstrate that thermally altered carbonaceous chondrites are plausible compositional analogs, however this is a tentative association due to a lack of prominent absorption features in our data. We have also conducted a series of high signal-to-noise visible-wavelength observations to investigate the reported surface heterogeneity. Our time series of visible spectra do not show variability at a precision level of a few percent. This result suggests two most likely possibilities. One, that the surface of 1999 JU3 is homogenous and that unaccounted for systematic effects are causing spectral variation across epochs. Or two, that the surface of 1999 JU3 is regionally heterogenous, in which case existing shape models suggest that any heterogeneity must be limited to terrains smaller than approximately 5% of the total surface area. These new observations represent the last opportunity before both the launch and return of the Hayabusa II spacecraft to perform ground-based characterization of this asteroid. Ultimately, these predictions for composition and surface properties will be tested upon completion of the mission. (C) 2013 Elsevier Inc. All rights reserved. C1 [Moskovitz, Nicholas A.; Pefkou, Dimitra; DeMeo, Francesca E.; Binzel, Richard P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Moskovitz, Nicholas A.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20008 USA. [Abe, Shinsuke; Pan, Kang-Shian] Natl Cent Univ, Inst Astron, Tao Yuan 32001, Taiwan. [Osip, David J.] Carnegie Inst Sci, Las Campanas Observ, La Serena, Chile. [Melita, Mario D.; Elias, Mauro] Univ Buenos Aires, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina. [Kitazato, Kohei] Univ Aizu, Res Ctr Adv Informat Sci & Technol, Aizu Wakamatsu, Fukushima 9658580, Japan. [Bus, Schelte J.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Abell, Paul A.] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. RP Moskovitz, NA (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM nmosko@mit.edu RI Melita, Mario /L-8624-2014 OI Melita, Mario /0000-0001-8128-0312 FU National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program [NNX-08AE38A]; Carnegie Institution of Washington Department of Terrestrial Magnetism; National Aeronautics and Space Administration through the NASA Astrobiology Institute (NAI) [NNA04CC09A]; National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship FX We are grateful to Vishnu Reddy and Faith Vilas for their insightful reviews. We thank David Polishook for his helpful input on the lightcurve analysis. This work includes data obtained at the Magellan 6.5 m telescopes located at Las Campanas Observatory in Chile and at NASA's IRTF located on Mauna Kea in Hawaii, which is operated by the University of Hawaii under Cooperative Agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. Support for this project was provided to N.M. by the Carnegie Institution of Washington Department of Terrestrial Magnetism, the National Aeronautics and Space Administration through the NASA Astrobiology Institute (NAI) under Cooperative Agreement No. NNA04CC09A, and through the National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship. NR 49 TC 14 Z9 14 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2013 VL 224 IS 1 BP 24 EP 31 DI 10.1016/j.icarus.2013.02.009 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133HC UT WOS:000318128500003 ER PT J AU Davidsson, BJR Gutierrez, PJ Groussin, O A'Hearn, MF Farnham, T Feaga, LM Kelley, MS Klaasen, KP Merlin, F Protopapa, S Rickman, H Sunshine, JM Thomas, PC AF Davidsson, Bjorn J. R. Gutierrez, Pedro J. Groussin, Olivier A'Hearn, Michael F. Farnham, Tony Feaga, Lori M. Kelley, Michael S. Klaasen, Kenneth P. Merlin, Frederic Protopapa, Silvia Rickman, Hans Sunshine, Jessica M. Thomas, Peter C. TI Thermal inertia and surface roughness of Comet 9P/Tempel 1 SO ICARUS LA English DT Article DE Comets, Nucleus; Thermal histories; Infrared observations ID DEEP IMPACT OBSERVATIONS; NUCLEUS PROPERTIES; SHAPE; CONDUCTIVITY; SPECTROSCOPY; TEMPERATURE; TOPOGRAPHY; ASTEROIDS; DENSITY; GEOLOGY AB Re-calibrated near-infrared spectroscopy of the resolved nucleus of Comet 9P/Tempel 1 acquired by the Deep Impact spacecraft has been analyzed by utilizing the post-Stardust-NExT nucleus shape model and spin pole solution, as well as a novel thermophysical model that explicitly accounts for small-scale surface roughness and thermal inertia. We find that the thermal inertia varies measurably across the surface, and that thermal emission from certain regions only can be reproduced satisfactory if surface roughness is accounted for. Particularly, a scarped/pitted terrain that experienced morning sunrise during the flyby is measurably rough (Hapke mean slope angle similar to 45 degrees) and has a thermal inertia of at most 50J m(-2) K-1 s(-1/2), but probably much lower. However, thick layered terrain and thin layered terrain experiencing local noon during the flyby have a substantially larger thermal inertia, reaching 150J m(-2) K-1 s(-1/2) if the surface is as rough as the scarped/pitted terrain, but 200J m(-2) K-1 s(-1/2) if the terrain is considered locally flat. Furthermore, the reddening of the nucleus near-infrared 1.5-2.2 gm spectrum varies between morphological units, being reddest for thick layered terrain (median value 3.4% k angstrom(-1)) and most neutral for the smooth terrain known to contain surface water ice (median value 3.1% k angstrom(-1)). Thus, Comet 9P/Tempel 1 is heterogeneous in terms of both thermophysical and optical properties, due to formation conditions and/or post-formation processing. (C) 2013 Elsevier Inc. All rights reserved. C1 [Davidsson, Bjorn J. R.; Rickman, Hans] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden. [Gutierrez, Pedro J.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Groussin, Olivier] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [A'Hearn, Michael F.; Farnham, Tony; Feaga, Lori M.; Kelley, Michael S.; Protopapa, Silvia; Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Klaasen, Kenneth P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Merlin, Frederic] Univ Paris 07, Observ Paris, LESIA, Sect Meudon 5, F-92195 Meudon, France. [Rickman, Hans] PAN Space Res Ctr, PL-00716 Warsaw, Poland. [Thomas, Peter C.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. RP Davidsson, BJR (reprint author), Uppsala Univ, Dept Phys & Astron, Box 516, SE-75120 Uppsala, Sweden. EM bjorn.davidsson@physics.uu.se; pedro-j@iaa.es; olivier.groussin@oamp.fr; ma@astro.umd.edu; farnham@astro.umd.edu; feaga@astro.umd.edu; msk@astro.umd.edu; kenneth.p.klaasen@jpl.nasa.gov; frederic.merlin@obspm.fr; protopapa@astro.umd.edu; hans.rickman@physics.uu.se; jess@astro.umd.edu; pct2@cornell.edu RI Gutierrez, Pedro/K-9637-2014; OI Gutierrez, Pedro/0000-0002-7332-6269; Kelley, Michael/0000-0002-6702-7676 FU Swedish National Space Board (SNSB) [96/09]; Faculty of Science and Technology at Uppsala University; NASA FX Davidsson is grateful for the financial support of the Swedish National Space Board (SNSB) which made this research possible (contract 96/09). Gutierrez acknowledges a guest researcher grant from the Faculty of Science and Technology at Uppsala University. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Support for the US-based investigators was provided by NASA both through the EPOXI project funded by NASA's Discovery Program and via various grants from NASA's Planetary Mission and Data Analysis Program. NR 37 TC 18 Z9 18 U1 0 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2013 VL 224 IS 1 BP 154 EP 171 DI 10.1016/j.icarus.2013.02.008 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133HC UT WOS:000318128500014 ER PT J AU Farnocchia, D Chesley, SR Chodas, PW Micheli, M Tholen, DJ Milani, A Elliott, GT Bernardi, F AF Farnocchia, D. Chesley, S. R. Chodas, P. W. Micheli, M. Tholen, D. J. Milani, A. Elliott, G. T. Bernardi, F. TI Yarkovsky-driven impact risk analysis for asteroid (99942) Apophis SO ICARUS LA English DT Article DE Asteroids, Dynamics; Celestial mechanics; Near-Earth objects; Orbit determination ID NEAR-EARTH ASTEROIDS; ENCOUNTERS AB We assess the risk of an Earth impact for asteroid (99942) Apophis by means of a statistical analysis accounting for the uncertainty of both the orbital solution and the Yarkovsky effect. We select those observations with either rigorous uncertainty information provided by the observer or a high established accuracy. For the Yarkovsky effect we perform a Monte Carlo simulation that fully accounts for the uncertainty in the physical characterization, especially for the unknown spin orientation. By mapping the uncertainty information onto the 2029 b-plane and identifying the keyholes corresponding to subsequent impacts we assess the impact risk for future encounters. In particular, we find an impact probability greater than 10(-6) for an impact in 2068. We analyze the stability of the impact probability with respect to the assumptions on Apophis' physical characterization and consider the possible effect of the early 2013 radar apparition. (C) 2013 Elsevier Inc. All rights reserved. C1 [Farnocchia, D.; Chesley, S. R.; Chodas, P. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Micheli, M.; Tholen, D. J.; Elliott, G. T.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Milani, A.] Univ Pisa, Dipartimento Matemat, I-56127 Pisa, Italy. [Bernardi, F.] SpaceDyS, I-56023 Pisa, Italy. RP Farnocchia, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Davide.Farnocchia@jpl.nasa.gov OI Micheli, Marco/0000-0001-7895-8209 FU NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology; NASA FX D.F. was supported for this research by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA.; S.C. and P.C. conducted this research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 37 TC 32 Z9 32 U1 2 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY PY 2013 VL 224 IS 1 BP 192 EP 200 DI 10.1016/j.icarus.2013.02.020 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133HC UT WOS:000318128500017 ER PT J AU Nixon, CA Teanby, NA Irwin, PGJ Horst, SM AF Nixon, Conor A. Teanby, Nicholas A. Irwin, Patrick G. J. Hoerst, Sarah M. TI Upper limits for PH3 and H2S in Titan's atmosphere from Cassini CIRS SO ICARUS LA English DT Article DE Titan; Abundances, Atmospheres; Atmospheres, Composition; Saturn, Satellites ID COMPOSITE INFRARED SPECTROMETER; ABUNDANCES; RATIOS AB We have searched for the presence of simple P and S-bearing molecules in Titan's atmosphere, by looking for the characteristic signatures of phosphine and hydrogen sulfide in infrared spectra obtained by Cassini CIRS. As a result we have placed the first upper limits on the stratospheric abundances, which are 1 ppb (PH3) and 330 ppb (H2S), at the 2-sigma significance level. Published by Elsevier Inc. C1 [Nixon, Conor A.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Teanby, Nicholas A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Irwin, Patrick G. J.] Univ Oxford, Oxford OX1 3PU, England. [Hoerst, Sarah M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Nixon, CA (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. EM conor.a.nixon@nasa.gov RI Horst, Sarah/A-9906-2010; Nixon, Conor/A-8531-2009; OI Horst, Sarah/0000-0003-4596-0702; Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X NR 19 TC 4 Z9 4 U1 0 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2013 VL 224 IS 1 BP 253 EP 256 DI 10.1016/j.icarus.2013.02.024 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133HC UT WOS:000318128500023 ER PT J AU Loeffler, MJ Hudson, RL AF Loeffler, Mark J. Hudson, Reggie L. TI Low-temperature thermal reactions between SO2 and H2O2 and their relevance to the jovian icy satellites SO ICARUS LA English DT Article DE Europa; Ices, IR spectroscopy; Jupiter, Satellites ID CRYSTALLINE WATER ICE; HYDROGEN-PEROXIDE; GALILEAN SATELLITES; ION IRRADIATION; SULFUR-DIOXIDE; EUROPA; SURFACE; UV; DECOMPOSITION; RADIOLYSIS AB Here we present first results on a non-radiolytic, thermally-driven reaction sequence in solid H2O + SO2 + H2O2 mixtures at 50-130 K, which produces sulfate (SO42-), and has an activation energy of 53 kJ/mole. We suspect that these results may explain some of the observations related to the presence and distribution of H2O2 across Europa's surface as well as the lack of H2O2 on Ganymede and Callisto. Published by Elsevier Inc. C1 [Loeffler, Mark J.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Branch, Greenbelt, MD 20771 USA. RP Loeffler, MJ (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Branch, Code 691, Greenbelt, MD 20771 USA. EM mark.loeffler@nasa.gov RI Loeffler, Mark/C-9477-2012 FU NASA; NASA Astrobiology Institute through the Goddard Center for Astrobiology FX The support of NASA's Planetary Geology and Geophysics program is gratefully acknowledged. R.L.H. also acknowledges support from the NASA Astrobiology Institute through the Goddard Center for Astrobiology. NR 29 TC 6 Z9 6 U1 3 U2 20 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2013 VL 224 IS 1 BP 257 EP 259 DI 10.1016/j.icarus.2013.02.005 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133HC UT WOS:000318128500024 ER PT J AU Namikawa, T Hanson, D Takahashi, R AF Namikawa, Toshiya Hanson, Duncan Takahashi, Ryuichi TI Bias-hardened CMB lensing SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; cosmic background radiation; cosmology: observations ID SOUTH-POLE TELESCOPE; COSMOLOGICAL SIMULATIONS; POWER SPECTRUM; MICROWAVE; RECONSTRUCTION; CONVERGENCE; MAPS; MODELS; PLANCK; CODE AB We present new methods for lensing reconstruction from CMB temperature fluctuations which have smaller mean-field and reconstruction noise bias corrections than current lensing estimators, with minimal loss of signal to noise. These biases are usually corrected using Monte Carlo simulations, and to the extent that these simulations do not perfectly mimic the underlying sky, there are uncertainties in the bias corrections. The bias-hardened estimators which we present can have reduced sensitivity to such uncertainties, and provide a desirable cross-check on standard results. To test our approach, we also show the results of lensing reconstruction from simulated temperature maps given on 10 x 10 deg(2), and confirm that our approach works well to reduce biases for a typical masked map in which 70 square masks each having 10 arcmin on a side exist, covering 2 per cent of the simulated map, which is similar to the masks used in the current SPT lensing analysis. C1 [Namikawa, Toshiya] Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan. [Hanson, Duncan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hanson, Duncan] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Takahashi, Ryuichi] Hirosaki Univ, Fac Sci & Technol, Hirosaki, Aomori 0368561, Japan. RP Namikawa, T (reprint author), Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan. EM namikawa.toshiya9@gmail.com RI Takahashi, Ryuichi/F-3362-2013; OI Namikawa, Toshiya/0000-0003-3070-9240 FU JSPS; Hirosaki University Grant for Exploratory Research by Young Scientists; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan; MEXT [21111006]; World Premier International Research Center Initiative (WPI Initiative) from MEXT of Japan; [467] FX We thank Aurelien Benoit-Levy, Karim Benabed, Ryo Nagata and Eiichiro Komatsu for useful comments and discussions, and greatly appreciate Takashi Hamana and Takahiro Nishimichi for kindly providing the ray-tracing simulation code and the 2LPT code. TN is also grateful to Atsushi Taruya for several comments and discussions. This work was supported in part by Grant-in-Aid for Scientific Research on Priority Areas No. 467 'Probing the Dark Energy through an Extremely Wide and Deep Survey with Subaru Telescope', JSPS Core-to-Core Programme 'International Research Network for Dark Energy', Hirosaki University Grant for Exploratory Research by Young Scientists, by the Grand-in-Aid for the Global COE Program 'Quest for Fundamental Principles in the Universe: from Particles to the Solar system and the Cosmos' from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan, by the MEXT Grant-in-Aid for Scientific Research on Innovative Areas (No. 21111006), by the FIRST program 'Subaru Measurements of Images and Redshifts (SuMIRe)', World Premier International Research Center Initiative (WPI Initiative) from MEXT of Japan. Numerical computations were carried out on SR16000 at YITP in Kyoto University and Cray XT4 at Center for Computational Astrophysics, CfCA, of National Astronomical Observatory of Japan. NR 52 TC 24 Z9 24 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 1 BP 609 EP 620 DI 10.1093/mnras/stt195 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136EE UT WOS:000318343600071 ER PT J AU Wang, L Farrah, D Oliver, SJ Amblard, A Bethermin, M Bock, J Conley, A Cooray, A Halpern, M Heinis, S Ibar, E Ilbert, O Ivison, RJ Marsden, G Roseboom, IG Rowan-Robinson, M Schulz, B Smith, AJ Viero, M Zemcov, M AF Wang, L. Farrah, D. Oliver, S. J. Amblard, A. Bethermin, M. Bock, J. Conley, A. Cooray, A. Halpern, M. Heinis, S. Ibar, E. Ilbert, O. Ivison, R. J. Marsden, G. Roseboom, I. G. Rowan-Robinson, M. Schulz, B. Smith, A. J. Viero, M. Zemcov, M. TI Connecting stellar mass and star-formation rate to dark matter halo mass out to z similar to 2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; cosmology: observations; large-scale structure of Universe; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; GALAXY FORMATION; PHOTOMETRIC REDSHIFTS; FORMATION HISTORY; LUMINOSITY DENSITY; COSMOS FIELD; SPITZER/IRAC SOURCES; FORMING GALAXIES AB We have constructed an extended halo model (EHM) which relates the total stellar mass and star-formation rate (SFR) to halo mass (M-h). An empirical relation between the distribution functions of total stellar mass of galaxies and host halo mass, tuned to match the spatial density of galaxies over 0 < z < 2 and the clustering properties at z similar to 0, is extended to include two different scenarios describing the variation of SFR on Mh. We also present new measurements of the redshift evolution of the average SFR for star-forming galaxies of different stellar masses up to z = 2, using data from the Herschel Multi-tiered Extragalactic Survey for infrared bright galaxies. Combining the EHM with the halo accretion histories from numerical simulations, we trace the stellar mass growth and star-formation history in haloes spanning a range of masses. We find that: (1) the intensity of the star-forming activity in haloes in the probed mass range has steadily decreased from z similar to 2 to 0; (2) at a given epoch, haloes in the mass range between a few times 10(11) M-circle dot and a few times 10(12) M-circle dot are the most efficient at hosting star formation; (3) the peak of SFR density shifts to lower mass haloes over time; and (4) galaxies that are forming stars most actively at z similar to 2 evolve into quiescent galaxies in today's group environments, strongly supporting previous claims that the most powerful starbursts at z similar to 2 are progenitors of today's elliptical galaxies. C1 [Wang, L.; Farrah, D.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Wang, L.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bethermin, M.] Univ Paris Diderot, CE Saclay, CNRS, Lab AIM Paris Saclay,CEA,DSM,Irfu, F-91191 Gif Sur Yvette, France. [Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France. [Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France. [Bock, J.; Cooray, A.; Schulz, B.; Viero, M.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Halpern, M.; Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Heinis, S.; Ilbert, O.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Schulz, B.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. RP Wang, L (reprint author), Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. EM lingyu.wang@sussex.ac.uk RI amblard, alexandre/L-7694-2014; Ivison, R./G-4450-2011; OI amblard, alexandre/0000-0002-2212-5395; Ivison, R./0000-0001-5118-1313; Bethermin, Matthieu/0000-0002-3915-2015 FU UK's Science and Technology Facilities Council [ST/F002858/1]; ERC StG grant [DEGAS-259586]; CSA (Canada); NAOC (China); CEA; CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA) FX LW acknowledges support from UK's Science and Technology Facilities Council grant ST/F002858/1 and an ERC StG grant (DEGAS-259586). SJO is supported by UK's Science and Technology Facilities Council grant ST/F002858/1. The data presented in this paper will be released through the Herschel data base in Marseille HeDaM (hedam.oamp.fr/herMES). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). NR 102 TC 38 Z9 38 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 1 BP 648 EP 661 DI 10.1093/mnras/stt190 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136EE UT WOS:000318343600074 ER PT J AU Matter, A Defrere, D Danchi, WC Lopez, B Absil, O AF Matter, A. Defrere, D. Danchi, W. C. Lopez, B. Absil, O. TI Parasitic interference in nulling interferometry SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; methods: analytical; techniques: interferometric ID EXOPLANET DETECTION; PERFORMANCE AB Nulling interferometry aims to detect faint objects close to bright stars. Its principle is to produce a destructive interference along the line of sight so that the stellar flux is rejected, while the flux of the off-axis source can be transmitted. In practice, various instrumental perturbations can degrade the nulling performance. Any imperfection in phase, amplitude or polarization produces a spurious flux that leaks to the interferometer output and corrupts the transmitted off-axis flux. One of these instrumental perturbations is the crosstalk phenomenon, which occurs because of multiple parasitic reflections inside transmitting optics, and/or diffraction effects related to beam propagation along finite size optics. It can include a crosstalk of a beam with itself, and a mutual crosstalk between different beams. This can create a parasitic interference pattern, which degrades the intrinsic transmission map - or intensity response - of the interferometer. In this context, we describe how this instrumental effect impairs the performance of a Bracewell interferometer. A simple formalism is developed to derive the corresponding modified intensity response of the interferometer, as a function of the two parameters of interest: the crosstalk level (or contamination rate) and the phase shift between the primary and secondary - parasitic - beams. We then apply our mathematical approach to a few scientific cases, both analytically and using the GENIESIM simulation software, adapted to handle coherent crosstalk. Our results show that a coherent crosstalk level of about 1 per cent implies a 20 per cent drop of the signal-to-noise ratio at most. Careful attention should thus be paid to reduce the crosstalk level inside an interferometric instrument and ensure an instrumental stability that provides the necessary sensitivity through calibration procedures. C1 [Matter, A.; Defrere, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Defrere, D.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Danchi, W. C.] NASA, GSFC, Greenbelt, MD 20771 USA. [Lopez, B.] UNS Observ Cote Azur, CNRS UMR 7293, Lab Lagrange, F-06304 Nice 4, France. [Absil, O.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium. RP Matter, A (reprint author), Inst Planetol & Astrophys Grenoble, 414 Rue Piscine,Domaine Univ, F-38400 St Martin Dheres, France. EM alexis.matter@obs.ujf-grenoble.fr OI Absil, Olivier/0000-0002-4006-6237 NR 13 TC 0 Z9 0 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 2 BP 1286 EP 1295 DI 10.1093/mnras/stt246 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136ER UT WOS:000318345200022 ER PT J AU Stacy, A Greif, TH Klessen, RS Bromm, V Loeb, A AF Stacy, Athena Greif, Thomas H. Klessen, Ralf S. Bromm, Volker Loeb, Abraham TI Rotation and internal structure of Population III protostars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; stars: Population III; galaxies: formation; cosmology: theory; dark ages, reionization, first stars; early Universe ID GAMMA-RAY BURSTS; PRIMORDIAL STAR-FORMATION; 1ST SUPERNOVA EXPLOSIONS; EARLY METAL ENRICHMENT; SMALL-SCALE DYNAMO; MASSIVE STARS; MAGNETIC-FIELDS; LOW-METALLICITY; PRESUPERNOVA EVOLUTION; PROTOSTELLAR COLLAPSE AB We analyse the cosmological simulations performed in the recent work of Greif et al., which followed the early growth and merger history of Population III (Pop III) stars while resolving scales as small as 0.05 R-circle dot. This is the first set of cosmological simulations to self-consistently resolve the rotation and internal structure of Pop III protostars. We find that Pop III stars form under significant rotational support which is maintained for the duration of the simulations. The protostellar surfaces spin from similar to 50 per cent to nearly 100 per cent of Keplerian rotational velocity. These rotation rates persist after experiencing multiple stellarmerger events. In the brief time period simulated (similar to 10 yr), the protostars show little indication of convective instability, and their properties furthermore show little correlation with the properties of their host minihaloes. If Pop III protostars within this range of environments generally form with high degrees of rotational support, and if this rotational support is maintained for a sufficient amount of time, this has a number of crucial implications for Pop III evolution and nucleosynthesis, as well as the possibility for Pop III pair-instability supernovae, and the question of whether the first stars produced gamma-ray bursts. C1 [Stacy, Athena] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Greif, Thomas H.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Greif, Thomas H.; Loeb, Abraham] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Klessen, Ralf S.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bromm, Volker] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA. RP Stacy, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM athena.stacy@nasa.gov FU JWST Postdoctoral Fellowship through the NASA Postdoctoral Program (NPP); NASA through Astrophysics Theory and Fundamental Physics Program [NNX09AJ33G]; NSF [AST-1009928] FX The authors wish to thank John Mather and Sally Heap for insightful discussions. AS is grateful for support from the JWST Postdoctoral Fellowship through the NASA Postdoctoral Program (NPP). VB acknowledges support from NASA through Astrophysics Theory and Fundamental Physics Program grant NNX09AJ33G and from NSF through grant AST-1009928. We acknowledge the contribution of Paul Clark, Simon Glover, Rowan Smith, Volker Springel and Naoki Yoshida in carrying out the simulations on which our analysis is based. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 124 TC 24 Z9 24 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 2 BP 1470 EP 1486 DI 10.1093/mnras/stt264 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136ER UT WOS:000318345200038 ER PT J AU Machida, MN Hosokawa, T AF Machida, Masahiro N. Hosokawa, Takashi TI Evolution of protostellar outflow around low-mass protostar SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; MHD; stars: formation; stars: low-mass; ISM: jets and outflows; ISM: magnetic fields ID MOLECULAR CLOUD CORES; 1ST HYDROSTATIC CORE; YOUNG STELLAR OBJECTS; ROTATING MAGNETIZED CLOUDS; STAR-FORMATION; NUMERICAL-CALCULATIONS; SUBMILLIMETER ARRAY; ISOTHERMAL CLOUDS; BIPOLAR OUTFLOWS; DISK ACCRETION AB The evolution of protostellar outflow is investigated with resistive magneto-hydrodynamic nested-grid simulations that cover a wide range of spatial scales (similar to 1 au-1 pc). We follow cloud evolution from the pre-stellar core stage until the infalling envelope dissipates long after the protostar formation. We also calculate protostellar evolution to derive protostellar luminosity with time-dependent mass accretion through a circumstellar disc. The protostellar outflow is driven by the first core prior to protostar formation and is directly driven by the circumstellar disc after protostar formation. The opening angle of the outflow is large in the Class 0 stage. A large fraction of the cloud mass is ejected in this stage, which reduces the star formation efficiency to similar to 50 per cent. After the outflow breaks out from the natal cloud, the outflow collimation is gradually improved in the Class I stage. The head of the outflow travels more than similar to 10(5) au in similar to 10(5) yr. The outflow momentum, energy and mass derived in our calculations agree well with observations. In addition, our simulations show the same correlations among outflow momentum flux, protostellar luminosity and envelope mass as those in observations. These correlations differ between Class 0 and I stages, which are explained by different evolutionary stages of the outflow; in the Class 0 stage, the outflow is powered by the accreting mass and acquires its momentum from the infalling envelope; in the Class I stage, the outflow enters the momentum-driven snow-plough phase. Our results suggest that protostellar outflow should determine the final stellar mass and significantly affect the early evolution of low-mass protostars. C1 [Machida, Masahiro N.] Kyushu Univ, Dept Earth & Planetary Sci, Fac Sci, Fukuoka 8128581, Japan. [Hosokawa, Takashi] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Hosokawa, Takashi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Machida, MN (reprint author), Kyushu Univ, Dept Earth & Planetary Sci, Fac Sci, Fukuoka 8128581, Japan. EM machida.masahiro.018@m.kyushu-u.ac.jp; takashi.hosokawa@phys.s.u-tokyo.ac.jp RI U-ID, Kyushu/C-5291-2016 NR 107 TC 25 Z9 25 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 2 BP 1719 EP 1744 DI 10.1093/mnras/stt291 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136ER UT WOS:000318345200057 ER PT J AU Agius, NK Sansom, AE Popescu, CC Andrae, E Baes, M Baldry, I Bourne, N Brough, S Clark, CJR Conselice, C Cooray, A Dariush, A De Zotti, G Driver, SP Dunne, L Eales, SA Foster, C Gomez, HL Haussler, B Hopkins, AM Hopwood, R Ivison, RJ Kelvin, LS Lara-Lopez, MA Liske, J Lopez-Sanchez, AR Loveday, J Maddox, S Madore, B Phillipps, S Robotham, A Rowlands, K Seibert, M Smith, MWL Temi, P Tuffs, R Valiante, E AF Agius, N. K. Sansom, A. E. Popescu, C. C. Andrae, E. Baes, M. Baldry, I. Bourne, N. Brough, S. Clark, C. J. R. Conselice, C. Cooray, A. Dariush, A. De Zotti, G. Driver, S. P. Dunne, L. Eales, S. A. Foster, C. Gomez, H. L. Haeussler, B. Hopkins, A. M. Hopwood, R. Ivison, R. J. Kelvin, L. S. Lara-Lopez, M. A. Liske, J. Lopez-Sanchez, A. R. Loveday, J. Maddox, S. Madore, B. Phillipps, S. Robotham, A. Rowlands, K. Seibert, M. Smith, M. W. L. Temi, P. Tuffs, R. Valiante, E. TI GAMA/H-ATLAS: linking the properties of submm detected and undetected early-type galaxies - I. z <= 0.06 sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; galaxies: elliptical and lenticular, cD; galaxies: evolution; submillimetre: galaxies ID MASS ASSEMBLY GAMA; DIGITAL SKY SURVEY; SCIENCE DEMONSTRATION PHASE; HERSCHEL REFERENCE SURVEY; NEARBY ELLIPTIC GALAXIES; STRONGLY LENSED GALAXIES; STAR-FORMATION; LENTICULAR GALAXIES; INTERSTELLAR MATTER; SAURON PROJECT AB We present two large, nearby (0.013 <= z <= 0.06) samples of early-type galaxies (ETGs): a visually classified sample of 220 ETGs, created using source-matched data from the Galaxy and Mass Assembly (GAMA) data base with far-infrared/submm detections from Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS); and a visually classified sample of 551 ETGs which are undetected with H-ATLAS. Active galactic nuclei are removed from our samples using optical emission-line diagnostics. These samples are scrutinized to determine characteristics of submm detected versus undetected ETGs. We find similarities in the stellar mass distributions of the two ETG samples but testing other properties uncovers significant differences. The submm detected sample is shown to have lower concentration and Sersic indices than those in the undetected sample - a result which may be linked to the presence of dust in the former. Optical and ultraviolet-optical colours are also shown to be much bluer, indicating that the dust is linked with recent star formation. The intrinsic effective radii are on average 1.5 times larger for the submm detected ETGs. Surface densities and groups data from the GAMA data base are examined for the two samples, leading to the conclusion that dusty ETGs inhabit sparser environments than non-dusty ETGs in the nearby Universe, although environments of the brightest ETGs are shown to differ the least. Modified Planck functions are fit to the H-ATLAS detected Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) fluxes for ETGs with submm flux densities of at least 3 sigma in the 350 mu m SPIRE band, giving a resultant mean cold dust temperature of T-d = 22.1 K, with a range of 9-30 K. The corresponding mean dust mass is 1.8 x 10(7) M-circle dot, with a range of (0.08-35.0) x 10(7) M-circle dot. The dust masses calculated from these fits, normalized by stellar mass, are shown to increase with decreasing stellar mass and bluer colours. Based on visual classifications of elliptical and lenticular, we find similar dust properties for these two early-type morphologies. We conclude that there is a population of elliptical galaxies which exhibit larger dust masses, lower Sersic index and bluer colours than the more well-known, massive, red population of ellipticals. C1 [Agius, N. K.; Sansom, A. E.; Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Andrae, E.; Tuffs, R.] Max Planck Inst Nucl Phys MPIK, D-69117 Heidelberg, Germany. [Baes, M.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Baldry, I.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Bourne, N.; Conselice, C.; Haeussler, B.; Rowlands, K.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Brough, S.; Hopkins, A. M.; Lara-Lopez, M. A.; Lopez-Sanchez, A. R.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Clark, C. J. R.; Eales, S. A.; Gomez, H. L.; Smith, M. W. L.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dariush, A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [De Zotti, G.] INAF Osservatorio Astron Padova, I-34136 Trieste, Italy. [De Zotti, G.] SISSA, I-34136 Trieste, Italy. [Driver, S. P.; Kelvin, L. S.; Robotham, A.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Driver, S. P.; Kelvin, L. S.; Robotham, A.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Foster, C.] European So Observ, Santiago 19, Chile. [Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Hopwood, R.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Sci & Technol Facil Council, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kelvin, L. S.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Liske, J.] European So Observ, D-85748 Garching, Germany. [Lopez-Sanchez, A. R.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Madore, B.; Seibert, M.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Phillipps, S.] Univ Bristol, Astrophys Grp, Sch Phys, Bristol BS8 1TL, Avon, England. [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. RP Agius, NK (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. EM nkagius@uclan.ac.uk RI Baes, Maarten/I-6985-2013; Robotham, Aaron/H-5733-2014; Driver, Simon/H-9115-2014; Ivison, R./G-4450-2011; OI Baes, Maarten/0000-0002-3930-2757; Robotham, Aaron/0000-0003-0429-3579; Driver, Simon/0000-0001-9491-7327; Ivison, R./0000-0001-5118-1313; Maddox, Stephen/0000-0001-5549-195X; Foster, Caroline/0000-0003-0247-1204; Liske, Jochen/0000-0001-7542-2927 FU Science and Technology Facilities Council; STFC (UK); ARC (Australia); AAO FX We would like to thank the anonymous referee whose comments led to important improvements in this paper. Additionally, we would like to thank Giovanni Natale for his comments and advice in the writing and proofing of this paper. NKA acknowledges the support of the Science and Technology Facilities Council. The Herschel-ATLAS is a project with Herschel; which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.h-atlas.org/. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programs including GALEX MIS, VST KIDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO and the participating institutions. The GAMA website is http://www.gama-survey.org/. NR 96 TC 13 Z9 13 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 2 BP 1929 EP 1946 DI 10.1093/mnras/stt310 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136ER UT WOS:000318345200073 ER PT J AU Marcolino, WLF Bouret, JC Sundqvist, JO Walborn, NR Fullerton, AW Howarth, ID Wade, GA Ud-Doula, A AF Marcolino, W. L. F. Bouret, J. -C. Sundqvist, J. O. Walborn, N. R. Fullerton, A. W. Howarth, I. D. Wade, G. A. Ud-Doula, A. TI Phase-resolved ultraviolet spectroscopy of the magnetic Of?p star HD 191612 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: atmospheres; stars: magnetic field; stars: massive ID O-STAR; HD-191612; SPECTRA; WINDS; FIELD; SIMULATIONS; REGIONS; FLOW AB We present for the first time phase-resolved ultraviolet (UV) spectroscopy of an Of? p star, namely, HD 191612. The observations were acquired with the Space Telescope Imaging Spectrograph (STIS) onboard the Hubble Space Telescope (HST). We report the variability observed in the main photospheric and wind features and compare the results with previous findings for the Of? p star HD 108. We show that UV line strengths, H alpha, and longitudinal magnetic field, vary coherently according to the rotational period (P-rot = 537.6 d), providing additional support for the magnetic oblique rotator scenario. The stellar and wind parameters of HD 191612 are obtained based on NLTE expanding atmosphere models. The peculiar wind line profile variations revealed by the new STIS data - not reproduced by 1D atmosphere models - are addressed through non-spherical magnetohydrodynamical simulations coupled with radiative transfer. The basic aspects of the UV variability observed are explained and the structure of the dynamical magnetosphere of HD 191612 is discussed. C1 [Marcolino, W. L. F.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil. [Bouret, J. -C.] CNRS, LAM UMR6110, F-13388 Marseille 13, France. [Bouret, J. -C.] Univ Aix Marseille 1, F-13388 Marseille 13, France. [Bouret, J. -C.] NASA, GSFC, Greenbelt, MD 20771 USA. [Sundqvist, J. O.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Walborn, N. R.; Fullerton, A. W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howarth, I. D.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Wade, G. A.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. [Ud-Doula, A.] Penn State Worthington Scranton, Dunmore, PA 18512 USA. RP Marcolino, WLF (reprint author), Univ Fed Rio de Janeiro, Observ Valongo, Ladeira Pedro Antonio 43, BR-20080090 Rio De Janeiro, Brazil. EM wagner@astro.ufrj.br RI Marcolino, Wagner/M-7428-2014 FU Fundacao de Amparo a Pesquisa do Estado do Rio de Janeiro (FAPERJ/APQ1); NASA [NNX08AC146, NAS5-26555]; NASA ATP grant [NNX11AC40G, NNX12AC72G]; NASA through STScI [GO-12179.01]; Natural Sciences and Engineering Research Council of Canada (NSERC); French Agence Nationale de la Recherche (ANR) FX WLFM acknowledges support from the Fundacao de Amparo a Pesquisa do Estado do Rio de Janeiro (FAPERJ/APQ1). JCB was supported by NASA grant NNX08AC146 to the University of Colorado at Boulder during the completion of this work. JOS acknowledges support from NASA ATP grant NNX11AC40G. NRW acknowledges support provided by NASA through grant GO-12179.01 from STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555. GAW acknowledges Discovery Grant support from the Natural Sciences and Engineering Research Council of Canada (NSERC). AuD acknowledges support from NASA ATP grant NNX12AC72G. We thank the French Agence Nationale de la Recherche (ANR) for financial support. NR 25 TC 9 Z9 9 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 3 BP 2253 EP 2260 DI 10.1093/mnras/stt323 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500018 ER PT J AU Symeonidis, M Vaccari, M Berta, S Page, MJ Lutz, D Arumugam, V Aussel, H Bock, J Boselli, A Buat, V Capak, PL Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Farrah, D Franceschini, A Giovannoli, E Glenn, J Griffin, M Hatziminaoglou, E Hwang, HS Ibar, E Ilbert, O Ivison, RJ Le Floc'h, E Lilly, S Kartaltepe, JS Magnelli, B Magdis, G Marchetti, L Nguyen, HT Nordon, R O'Halloran, B Oliver, SJ Omont, A Papageorgiou, A Patel, H Pearson, CP Perez-Fournon, I Pohlen, M Popesso, P Pozzi, F Rigopoulou, D Riguccini, L Rosario, D Roseboom, IG Rowan-Robinson, M Salvato, M Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Valtchanov, I Wang, L Xu, CK Zemcov, M Wuyts, S AF Symeonidis, M. Vaccari, M. Berta, S. Page, M. J. Lutz, D. Arumugam, V. Aussel, H. Bock, J. Boselli, A. Buat, V. Capak, P. L. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Farrah, D. Franceschini, A. Giovannoli, E. Glenn, J. Griffin, M. Hatziminaoglou, E. Hwang, H. -S. Ibar, E. Ilbert, O. Ivison, R. J. Le Floc'h, E. Lilly, S. Kartaltepe, J. S. Magnelli, B. Magdis, G. Marchetti, L. Nguyen, H. T. Nordon, R. O'Halloran, B. Oliver, S. J. Omont, A. Papageorgiou, A. Patel, H. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Popesso, P. Pozzi, F. Rigopoulou, D. Riguccini, L. Rosario, D. Roseboom, I. G. Rowan-Robinson, M. Salvato, M. Schulz, B. Scott, Douglas Seymour, N. Shupe, D. L. Smith, A. J. Valtchanov, I. Wang, L. Xu, C. K. Zemcov, M. Wuyts, S. TI The Herschel census of infrared SEDs through cosmic time SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimetre: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; SIMILAR-TO 2; HUBBLE-DEEP-FIELD; DEGREE EXTRAGALACTIC SURVEY; HIGH-REDSHIFT GALAXIES; MU-M OBSERVATIONS; SUBMILLIMETER GALAXIES AB Using Herschel data from the deepest SPIRE and PACS surveys (HerMES and PEP) in COSMOS, GOODS-S and GOODS-N, we examine the dust properties of infrared (IR)-luminous (L-IR > 10(10) L-circle dot) galaxies at 0.1 < z < 2 and determine how these evolve with cosmic time. The unique angle of this work is the rigorous analysis of survey selection effects, making this the first study of the star-formation-dominated, IR-luminous population within a framework almost entirely free of selection biases. We find that IR-luminous galaxies have spectral energy distributions (SEDs) with broad far-IR peaks characterized by cool/extended dust emission and average dust temperatures in the 25-45 K range. Hot (T > 45 K) SEDs and cold (T < 25 K), cirrus-dominated SEDs are rare, with most sources being within the range occupied by warm starbursts such as M82 and cool spirals such as M51. We observe a luminosity-temperature (L-T) relation, where the average dust temperature of log [L-IR/L-circle dot] similar to 12.5 galaxies is about 10 K higher than that of their log [L-IR/L-circle dot] similar to 10.5 counterparts. However, although the increased dust heating in more luminous systems is the driving factor behind the L-T relation, the increase in dust mass and/or starburst size with luminosity plays a dominant role in shaping it. Our results show that the dust conditions in IR-luminous sources evolve with cosmic time: at high redshift, dust temperatures are on average up to 10 K lower than what is measured locally (z less than or similar to 0.1). This is manifested as a flattening of the L-T relation, suggesting that (ultra) luminous infrared galaxies [(U)LIRGs] in the early Universe are typically characterized by a more extended dust distribution and/or higher dust masses than local equivalent sources. Interestingly, the evolution in dust temperature is luminosity dependent, with the fraction of LIRGs with T < 35 K showing a two-fold increase from z similar to 0 to z similar to 2, whereas that of ULIRGs with T < 35 K shows a six-fold increase. Our results suggest a greater diversity in the IR-luminous population at high redshift, particularly for ULIRGs. C1 [Symeonidis, M.; Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Vaccari, M.; Franceschini, A.; Marchetti, L.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Vaccari, M.; Giovannoli, E.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa. [Berta, S.; Lutz, D.; Magnelli, B.; Popesso, P.; Rosario, D.; Wuyts, S.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Arumugam, V.; Ivison, R. J.; Roseboom, I. G.] Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Aussel, H.; Boselli, A.; Le Floc'h, E.] Univ Paris Diderot, CNRS, CE Saclay, Lab AIM Paris Saclay,CEA DSM Irfu, F-91191 Gif Sur Yvette, France. [Bock, J.; Capak, P. L.; Cooray, A.; Dowell, C. D.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Buat, V.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Clements, D. L.; O'Halloran, B.; Patel, H.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Riguccini, L.; Valtchanov, I.] Villanueva Canada, European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Glenn, J.] Univ Colorado, CASA UCB 389, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Griffin, M.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Hwang, H. -S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ilbert, O.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13376 Marseille 12, France. [Lilly, S.] Inst Astron, CH-8093 Zurich, Switzerland. [Kartaltepe, J. S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Magdis, G.; Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Nordon, R.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Omont, A.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Perez-Fournon, I.] IAC, E-38200 Tenerife, Spain. [Perez-Fournon, I.] ULL, Departamento Astrofis, E-38205 Tenerife, Spain. [Pozzi, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Riguccini, L.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Salvato, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. RP Symeonidis, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM m.symeonidis@ucl.ac.uk RI Magdis, Georgios/C-7295-2014; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; OI Magdis, Georgios/0000-0002-4872-2294; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536 FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX This paper uses data from Herschel's photometers SPIRE and PACS. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). NR 161 TC 78 Z9 78 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 3 BP 2317 EP 2340 DI 10.1093/mnras/stt330 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500024 ER PT J AU Creevey, OL Thevenin, F Basu, S Chaplin, WJ Bigot, L Elsworth, Y Huber, D Monteiro, MJPFG Serenelli, A AF Creevey, O. L. Thevenin, F. Basu, S. Chaplin, W. J. Bigot, L. Elsworth, Y. Huber, D. Monteiro, M. J. P. F. G. Serenelli, A. TI A large sample of calibration stars for Gaia: log g from Kepler and CoRoT fields SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; stars: fundamental parameters; stars: solar-type; Galaxy: fundamental parameters ID SOLAR-LIKE OSCILLATIONS; ALPHA-CENTAURI-B; STELLAR EVOLUTION CODE; EQUATION-OF-STATE; SUN-LIKE STAR; FUNDAMENTAL PROPERTIES; MAIN-SEQUENCE; RED GIANTS; ASTEROSEISMIC ANALYSIS; ECLIPSING BINARY AB Asteroseismic data can be used to determine stellar surface gravities with precisions of <0.05 dex by using the global seismic quantities and nu(max) along with standard atmospheric data such as T-eff and metallicity. Surface gravity is also one of the four stellar properties to be derived by automatic analyses for one billion stars from Gaia data (work-package GSP_PHOT). In this paper, we explore seismic data from main-sequence F, G, K stars (solar-like stars) observed by the Kepler spacecraft as a potential calibration source for the methods that Gaia will use for object characterization (log g). We calculate log g for some bright nearby stars for which radii and masses are known (e. g. from interferometry or binaries), and using their global seismic quantities in a grid-based method, we determine an asteroseismic log g to within 0.01 dex of the direct calculation, thus validating the accuracy of our method. We also find that errors in adopted atmospheric parameters (mainly [Fe/H]) can, however, cause systematic errors of the order of 0.02 dex. We then apply our method to a list of 40 stars to deliver precise values of surface gravity, i.e. uncertainties of the order of 0.02 dex, and we find agreement with recent literature values. Finally, we explore the typical precision that we expect in a sample of more than 400 Kepler stars which have their global seismic quantities measured. We find a mean uncertainty (precision) of the order of better than 0.02 dex in log g over the full explored range 3.8 < log g < 4.6, with the mean value varying only with stellar magnitude (0.01-0.02 dex). We study sources of systematic errors in log g and find possible biases of the order of 0.04 dex, independent of log g and magnitude, which accounts for errors in the T-eff and [Fe/H] measurements, as well as from using a different grid-based method. We conclude that Kepler stars provide a wealth of reliable information that can help to calibrate methods that Gaia will use, in particular, for source characterization with GSP_PHOT, where excellent precision (small uncertainties) and accuracy in log g is obtained from seismic data. C1 [Creevey, O. L.; Thevenin, F.; Bigot, L.] Univ Nice Sophia Antipolis, CNRS, Lab Lagrange, F-06300 Nice, France. [Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Chaplin, W. J.; Elsworth, Y.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Monteiro, M. J. P. F. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Monteiro, M. J. P. F. G.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal. [Serenelli, A.] Fac Ciencias, IEEC, CSIC, Inst Space Sci, Bellaterra, Spain. RP Creevey, OL (reprint author), Univ Nice Sophia Antipolis, CNRS, Lab Lagrange, F-06300 Nice, France. EM ocreevey@oca.eu RI Monteiro, Mario J.P.F.G./B-4715-2008; Basu, Sarbani/B-8015-2014; OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Basu, Sarbani/0000-0002-6163-3472; Serenelli, Aldo/0000-0001-6359-2769 FU NSF [AST-1105930]; European Union [PIRG-GA-2009-247732]; MICINN [AYA2011-24704]; ESF EUROCORES Program EuroGENE-SIS [EUI2009-04170]; SGR; EU-FEDER; UK STFC; FCT/MEC (Portugal) [PTDC/CTE-AST/098754/2008]; FEDER (EC); OCA; Conseil General des Alpes-Maritimes FX OLC thanks Luca Casagrande and Victor Silva Aguirre for making data available. SB acknowledges NSF grant AST-1105930. AMS is supported in part by the European Union International Reintegration Grant PIRG-GA-2009-247732, the MICINN grant AYA2011-24704, by the ESF EUROCORES Program EuroGENE-SIS (MICINN grant EUI2009-04170), by SGR grants of the Generalitat de Catalunya and by the EU-FEDER funds. WJC and YE thank the UK STFC for grant funding to support asteroseismic research. MJPFGM acknowledges the support through research grant PTDC/CTE-AST/098754/2008, from FCT/MEC (Portugal) and FEDER (EC). OLC is a Henri Poincare Fellow at the Observatoire de la Cote d'Azur (OCA), funded by OCA and the Conseil General des Alpes-Maritimes. NR 134 TC 27 Z9 27 U1 1 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 3 BP 2419 EP 2432 DI 10.1093/mnras/stt336 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500032 ER PT J AU D'Ammando, F Antolini, E Tosti, G Finke, J Ciprini, S Larsson, S Ajello, M Covino, S Gasparrini, D Gurwell, M Hauser, M Romano, P Schinzel, F Wagner, SJ Impiombato, D Perri, M Persic, M Pian, E Polenta, G Sbarufatti, B Treves, A Vercellone, S Wehrle, A Zook, A AF D'Ammando, F. Antolini, E. Tosti, G. Finke, J. Ciprini, S. Larsson, S. Ajello, M. Covino, S. Gasparrini, D. Gurwell, M. Hauser, M. Romano, P. Schinzel, F. Wagner, S. J. Impiombato, D. Perri, M. Persic, M. Pian, E. Polenta, G. Sbarufatti, B. Treves, A. Vercellone, S. Wehrle, A. Zook, A. TI Long-term monitoring of PKS 0537-441 with Fermi-LAT and multiwavelength observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; BL Lacertae objects: general; BL Lacertae objects: individual: PKS 0537-441; galaxies: quasars: general ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; SOUTHERN RADIO-SOURCES; BLAZAR 3C 454.3; GAMMA-RAY; COMPLETE SAMPLE; MULTIFREQUENCY OBSERVATIONS; ENERGY-DISTRIBUTION AB We report on multiwavelength observations of the blazar PKS 0537-441 (z = 0.896) obtained from microwaves through gamma-rays by Submillimeter Array, Rapid Eye Mounting, Automatic Telescope for Optical Monitoring (ATOM), Swift and Fermi mostly during 2008 August-2010 April. Strong variability has been observed in gamma-rays, with two major flaring episodes (2009 July and 2010 March) and a harder-when-brighter behaviour, quite common for flat spectrum radio quasars and low-synchrotron-peaked BL Lacertae objects (BL Lacs), in 2010 March. In the same way, the spectral energy distribution (SED) of the source cannot be modelled by a simple synchrotron self-Compton model, as opposed to many BL Lacs, but the addition of an external Compton component of seed photons from a dust torus is needed. The 230 GHz light curve showed an increase simultaneous with the gamma-ray one, indicating co-spatiality of the mm and gamma-ray emission region likely at large distance from the central engine. The low, average, and high activity SED of the source could be fit changing only the electron distribution parameters, but two breaks in the electron distribution are necessary. The ensuing extra spectral break, located at near-infrared (NIR)-optical frequencies, together with that in gamma-rays seem to indicate a common origin, most likely due to an intrinsic feature in the underlying electron distribution. An overall correlation between the gamma-ray band with the R band and K band has been observed with no significant time lag. On the other hand, when inspecting the light curves on short time-scales some differences are evident. In particular, flaring activity has been detected in NIR and optical bands with no evident gamma-ray counterparts in 2009 September and November. Moderate variability has been observed in X-rays with no correlation between flux and photon index. An increase of the detected X-ray flux with no counterpart at the other wavelengths has been observed in 2008 October, suggesting once more a complex correlation between the emission at different energy bands. C1 [D'Ammando, F.; Antolini, E.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [D'Ammando, F.; Antolini, E.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Finke, J.] USN, Res Lab, Washington, DC 20375 USA. [Ciprini, S.; Gasparrini, D.; Perri, M.; Polenta, G.] ASI, Sci Data Ctr, I-00044 Rome, Italy. [Larsson, S.] Stockholm Univ, Albanova, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Albanova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Ajello, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ajello, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ajello, M.; Sbarufatti, B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Covino, S.] Oss Astron Brera, INAF, I-23807 Merate, LC, Italy. [Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hauser, M.; Wagner, S. J.] Heidelberg Univ, Landerssternwarte, D-69117 Heidelberg, Germany. [Romano, P.; Impiombato, D.; Vercellone, S.] IASF Palermo, INAF, I-90146 Palermo, Italy. [Schinzel, F.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Persic, M.; Pian, E.] OA Trieste, INAF, I-34127 Trieste, Italy. [Persic, M.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Polenta, G.] Oss Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Sbarufatti, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Treves, A.] Univ Insubria, Dept Math & Phys, I-22100 Como, Italy. [Wehrle, A.] Space Sci Inst, Boulder, CO 80301 USA. [Zook, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP D'Ammando, F (reprint author), Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. EM dammando@ira.inaf.it OI Vercellone, Stefano/0000-0003-1163-1396; Perri, Matteo/0000-0003-3613-4409; Polenta, Gianluca/0000-0003-4067-9196; Persic, Massimo/0000-0003-1853-4900; Sbarufatti, Boris/0000-0001-6620-8347; Covino, Stefano/0000-0001-9078-5507; Gasparrini, Dario/0000-0002-5064-9495; Pian, Elena/0000-0001-8646-4858 FU Smithsonian Institution; Academia Sinica; National Aeronautics and Space Administration; ESA Member States; NASA; PRIN-INAF FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We thank the Swift team for making these observations possible, the duty scientists and science planners. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This paper is partly based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. We thank the anonymous referee, Y. Tanaka, C. Dermer, S. Digel, and E. Charles for useful comments and suggestions. Some authors acknowledge financial contribution from grant PRIN-INAF-2011. NR 93 TC 21 Z9 21 U1 1 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 3 BP 2481 EP 2492 DI 10.1093/mnras/stt344 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500038 ER PT J AU Todling, R AF Todling, Ricardo TI Comparing Two Approaches for Assessing Observation Impact SO MONTHLY WEATHER REVIEW LA English DT Article ID VARIATIONAL DATA ASSIMILATION; ANALYSIS SYSTEM; OBSERVATION SENSITIVITY; KALMAN FILTER; PART I; ADJOINT; MODEL; ERROR; IMPLEMENTATION; APPROXIMATIONS AB Langland and Baker introduced an approach to assess the impact of observations on the forecasts. In that approach, a state-space aspect of the forecast is defined and a procedure is derived ultimately relating changes in the aspect with changes in the observing system. Some features of the state-space approach are to be noted: the typical choice of forecast aspect is rather subjective and leads to incomplete assessment of the observing system, it requires availability of a verification state that is in practice correlated with the forecast, and it involves the adjoint operator of the entire data assimilation system and is thus constrained by the validity of this operator. This article revisits the topic of observation impacts from the perspective of estimation theory. An observation-space metric is used to allow inferring observation impact on the forecasts without the limitations just mentioned. Using differences of observation-minus-forecast residuals obtained from consecutive forecasts leads to the following advantages: (i) it suggests a rather natural choice of forecast aspect that directly links to the data assimilation procedure, (ii) it avoids introducing undesirable correlations in the forecast aspect since verification is done against the observations, and (iii) it does not involve linearization and use of adjoints. The observation-space approach has the additional advantage of being nearly cost free and very simple to implement. In its simplest form it reduces to evaluating the statistics of observation-minus-background and observation-minus-analysis residuals with traditional methods. Illustrations comparing the approaches are given using the NASA Goddard Earth Observing System. C1 NASA, Global Modeling & Assimilat Off, GSFC, Greenbelt, MD 20771 USA. RP Todling, R (reprint author), NASA, Global Modeling & Assimilat Off, GSFC, Code 610-1, Greenbelt, MD 20771 USA. EM ricardo.todling@nasa.gov FU Atmospheric Data Assimilation Development component of the NASA Modeling, Analysis and Prediction Program [MAP/04-0000-0080] FX The author would like to thank Stephen E. Cohn for fruitful discussions at different stages of this work, and for having gone over an early version of this manuscript. The author also thanks Dacian N. Daescu for discussions at an early stage of this investigation. Thanks are also due to two anonymous reviewers for providing insightful comments and helping to improve the arguments presented in this study, and to Herschel Mitchell for helping improve readability. The computational work was carried out on the Linux Explore and Discover Systems through co-operation with the NASA Center for Computational Sciences at Goddard Space Flight Center. This research was partially supported by the Atmospheric Data Assimilation Development component of the NASA Modeling, Analysis and Prediction Program (MAP/04-0000-0080). NR 53 TC 7 Z9 7 U1 0 U2 3 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 MAY PY 2013 VL 141 IS 5 BP 1484 EP 1505 DI 10.1175/MWR-D-12-00100.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 137SW UT WOS:000318458700006 ER PT J AU Das, I Bell, RE Scambos, TA Wolovick, M Creyts, TT Studinger, M Frearson, N Nicolas, JP Lenaerts, JTM van den Broeke, MR AF Das, Indrani Bell, Robin E. Scambos, Ted A. Wolovick, Michael Creyts, Timothy T. Studinger, Michael Frearson, Nicholas Nicolas, Julien P. Lenaerts, Jan T. M. van den Broeke, Michiel R. TI Influence of persistent wind scour on the surface mass balance of Antarctica SO NATURE GEOSCIENCE LA English DT Article ID EAST ANTARCTICA; SNOW ACCUMULATION; VARIABILITY; PLATEAU; RADAR; AREAS; MODEL AB Accurate quantification of surface snow accumulation over Antarctica is a key constraint for estimates of the Antarctic mass balance, as well as climatic interpretations of ice-core records(1,2). Over Antarctica, near-surface winds accelerate down relatively steep surface slopes, eroding and sublimating the snow. This wind scour results in numerous localized regions (<= 200 km(2)) with reduced surface accumulation(3-7). Estimates of Antarctic surface mass balance rely on sparse point measurements or coarse atmospheric models that do not capture these local processes, and overestimate the net mass input in wind-scour zones(3). Here we combine airborne radar observations of unconformable stratigraphic layers with lidar-derived surface roughness measurements to identify extensive wind-scour zones over Dome A, in the interior of East Antarctica. The scour zones are persistent because they are controlled by bedrock topography. On the basis of our Dome A observations, we develop an empirical model to predict wind-scour zones across the Antarctic continent and find that these zones are predominantly located in East Antarctica. We estimate that similar to 2.7-6.6% of the surface area of Antarctica has persistent negative net accumulation due to wind scour, which suggests that, across the continent, the snow mass input is overestimated by 11-36.5 Gt yr(-1) in present surface-mass-balance calculations. C1 [Das, Indrani; Bell, Robin E.; Wolovick, Michael; Creyts, Timothy T.; Frearson, Nicholas] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Scambos, Ted A.] Univ Colorado, CIRES, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Studinger, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nicolas, Julien P.] Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, Columbus, OH 43210 USA. [Nicolas, Julien P.] Ohio State Univ, Atmospher Sci Program, Columbus, OH 43210 USA. [Lenaerts, Jan T. M.; van den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, NL-3584 CC Utrecht, Netherlands. RP Das, I (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. EM indrani@ldeo.columbia.edu RI Van den Broeke, Michiel/F-7867-2011; Lenaerts, Jan/D-9423-2012 OI Van den Broeke, Michiel/0000-0003-4662-7565; Lenaerts, Jan/0000-0003-4309-4011 FU AGAP-NSF [0632292]; RL-NSF [0636883]; IceBridge-NASA [NNNX11AC22G]; NSF-OPP [0538103]; [NASA-NNX10AL42G] FX This work was supported by AGAP-NSF 0632292 (R.E.B., T.T.C., I.D., M.W.), RL-NSF 0636883 (R.E.B., I.D.), IceBridge-NASA NNNX11AC22G (R.E.B.), NSF-OPP 0538103 (T.A.S.) and NASA-NNX10AL42G (T.A.S.). We thank R. Hock, C. Shuman and R. Buck for early reviews of the paper. S. Arcone is acknowledged for helpful discussions. T. Haran, A. Block and H. Abdi are acknowledged for their help in data processing and GIS (geographic information system) support. NR 29 TC 26 Z9 27 U1 1 U2 17 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD MAY PY 2013 VL 6 IS 5 BP 367 EP 371 DI 10.1038/NGEO1766 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 134QA UT WOS:000318227000016 ER PT J AU Steig, EJ Ding, QH White, JWC Kuttel, M Rupper, SB Neumann, TA Neff, PD Gallant, AJE Mayewski, PA Taylor, KC Hoffmann, G Dixon, DA Schoenemann, SW Markle, BR Fudge, TJ Schneider, DP Schauer, AJ Teel, RP Vaughn, BH Burgener, L Williams, J Korotkikh, E AF Steig, Eric J. Ding, Qinghua White, James W. C. Kuettel, Marcel Rupper, Summer B. Neumann, Thomas A. Neff, Peter D. Gallant, Ailie J. E. Mayewski, Paul A. Taylor, Kendrick C. Hoffmann, Georg Dixon, Daniel A. Schoenemann, Spruce W. Markle, Bradley R. Fudge, Tyler J. Schneider, David P. Schauer, Andrew J. Teel, Rebecca P. Vaughn, Bruce H. Burgener, Landon Williams, Jessica Korotkikh, Elena TI Recent climate and ice-sheet changes in West Antarctica compared with the past 2,000 years SO NATURE GEOSCIENCE LA English DT Article ID PACIFIC-OCEAN; EL-NINO; VARIABILITY; RECORD; PROXY; CORE; TEMPERATURE; CIRCULATION; GLACIER; TROPICS AB Changes in atmospheric circulation over the past five decades have enhanced the wind-driven inflow of warm ocean water onto the Antarctic continental shelf, where it melts ice shelves from below(1-3). Atmospheric circulation changes have also caused rapid warming(4) over the West Antarctic Ice Sheet, and contributed to declining sea-ice cover in the adjacent Amundsen-Bellingshausen seas(5). It is unknown whether these changes are part of a longer-term trend. Here, we use water-isotope (delta O-18) data from an array of ice-core records to place recent West Antarctic climate changes in the context of the past two millennia. We find that the delta O-18 of West Antarctic precipitation has increased significantly in the past 50 years, in parallel with the trend in temperature, and was probably more elevated during the 1990s than at any other time during the past 200 years. However, delta O-18 anomalies comparable to those of recent decades occur about 1% of the time over the past 2,000 years. General circulation model simulations suggest that recent trends in delta O-18 and climate in West Antarctica cannot be distinguished from decadal variability that originates in the tropics. We conclude that the uncertain trajectory of tropical climate variability represents a significant source of uncertainty in projections of West Antarctic climate and ice-sheet change. C1 [Steig, Eric J.; Ding, Qinghua; Kuettel, Marcel; Neff, Peter D.; Gallant, Ailie J. E.; Schoenemann, Spruce W.; Markle, Bradley R.; Fudge, Tyler J.; Schauer, Andrew J.; Teel, Rebecca P.] Univ Washington, Quaternary Res Ctr, Seattle, WA 98195 USA. [Steig, Eric J.; Ding, Qinghua; Kuettel, Marcel; Neff, Peter D.; Gallant, Ailie J. E.; Schoenemann, Spruce W.; Markle, Bradley R.; Fudge, Tyler J.; Schauer, Andrew J.; Teel, Rebecca P.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [White, James W. C.; Vaughn, Bruce H.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80303 USA. [Rupper, Summer B.; Burgener, Landon; Williams, Jessica] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. [Neumann, Thomas A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Mayewski, Paul A.; Dixon, Daniel A.; Korotkikh, Elena] Univ Maine, Climate Change Inst, Orono, ME 04469 USA. [Mayewski, Paul A.; Dixon, Daniel A.; Korotkikh, Elena] Univ Maine, Sch Earth & Climate Sci, Orono, ME 04469 USA. [Taylor, Kendrick C.] Univ Nevada, Desert Res Inst, Reno, NV 89512 USA. [Hoffmann, Georg] Ctr Etud Saclay, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. [Hoffmann, Georg] Univ Utrecht, Inst Marine & Atmospher Res, NL-3508 TC Utrecht, Netherlands. [Schneider, David P.] Natl Ctr Atmospher Res, Boulder, CO 80305 USA. RP Steig, EJ (reprint author), Univ Washington, Quaternary Res Ctr, Seattle, WA 98195 USA. EM steig@uw.edu RI White, James/A-7845-2009; Neff, Peter/B-3542-2014; Neumann, Thomas/D-5264-2012; Gallant, Ailie/N-3938-2013; Schneider, David/E-2726-2010; ding, qinghua/G-1186-2011; Steig, Eric/G-9088-2015; Taylor, Kendrick/A-3469-2016; OI VAUGHN, BRUCE/0000-0001-6503-957X; White, James/0000-0001-6041-4684; Steig, Eric/0000-0002-8191-5549; Taylor, Kendrick/0000-0001-8535-1261; Rupper, Summer/0000-0001-8655-5282 FU National Science Foundation Office of Polar Programs [0537930, 0837988, 0963924, 1043092, 05379853, 1043167, 0944730, 0230396, 0440817, 0944348, 0944266, 0096305, 9316564, 0096299, 0424589, 0439589, 063740, 063650, 0837883, 0838871]; National Science Foundation FX This work was supported by the National Science Foundation Office of Polar Programs (grant numbers 0537930, 0837988, 0963924 and 1043092 to E.J.S.; 05379853 and 1043167 to J.W.C.W.; 0944730 to S.B.R.; 0230396, 0440817, 0944348 and 0944266 to K.C.T.; 0096305, 9316564, 0096299, 0424589, 0439589, 063740, 063650 and 0837883 to P.A.M.; 0838871 to D.P.S.). NCAR is sponsored by the National Science Foundation. We thank A. Orsi, J. Bautista and J. Flaherty. NR 30 TC 44 Z9 44 U1 0 U2 86 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD MAY PY 2013 VL 6 IS 5 BP 372 EP 375 DI 10.1038/NGEO1778 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 134QA UT WOS:000318227000017 ER PT J AU Wang, B Hirose, N Moon, JH Yuan, DL AF Wang, Bin Hirose, Naoki Moon, Jae-Hong Yuan, Dongliang TI Difference between the Lagrangian trajectories and Eulerian residual velocity fields in the southwestern Yellow Sea SO OCEAN DYNAMICS LA English DT Article DE Eulerian residual velocity; Eulerian tidal residual current; Yellow Sea; Lagrangian drifter; Bottom friction parameterization ID EAST CHINA SEAS; STRATIFIED TIDAL RECTIFICATION; FINITE-AMPLITUDE BANKS; MEAN CIRCULATION; CURRENTS; MODEL; ESTUARIES; ADVECTION; MASS AB The responses to tidal and/or wind forces of Lagrangian trajectories and Eulerian residual velocity in the southwestern Yellow Sea are investigated using a high-resolution circulation model. The simulated tidal harmonic constants agree well with observations and existing studies. The numerical experiment reproduces the long-range southeastward Eulerian residual current over the sloping bottom around the Yangtze Bank also shown in previous studies. However, the modeled drifters deployed at the northeastern flank of the Yangtze Bank in the simulation move northeastward, crossing over this strong southeastward Eulerian residual current rather than following it. Additional sensitivity experiments reveal that the influence of the Eulerian tidal residual currents on Lagrangian trajectories is relatively weaker than that of the wind driven currents. This result is consistent with the northeastward movement of ARGOS surface drifters actually released in the southwestern Yellow Sea. Further experiments suggest that the quadratic nature of the bottom friction is the crucial factor, in the southwestern Yellow Sea, for the weaker influence of the Eulerian tidal residual currents on the Lagrangian trajectories. This study demonstrates that the Lagrangian trajectories do not follow the Eulerian residual velocity fields in the shallow coastal regions of the southwestern Yellow Sea. C1 [Wang, Bin; Hirose, Naoki] Kyushu Univ, Interdisciplinary Grad Sch Engn Sci, Dept Earth Syst Sci & Technol, Kasuga, Fukuoka 816, Japan. [Hirose, Naoki] Kyushu Univ, Appl Mech Res Inst, Kasuga, Fukuoka 816, Japan. [Moon, Jae-Hong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Yuan, Dongliang] Chinese Acad Sci, Key Lab Ocean Circulat & Wave, Qingdao, Peoples R China. [Yuan, Dongliang] Chinese Acad Sci, Inst Oceanol, Qingdao, Peoples R China. RP Wang, B (reprint author), Kyushu Univ, Interdisciplinary Grad Sch Engn Sci, Dept Earth Syst Sci & Technol, Kasuga, Fukuoka 816, Japan. EM wangbin@riam.kyushu-u.ac.jp RI Kyushu, RIAM/F-4018-2015; U-ID, Kyushu/C-5291-2016 FU MEXT/JSPS FX This work is supported by the MEXT/JSPS Grant-in-Aid for Young Scientists (A) program. The authors thank the Asia-Pacific Data Research Center for providing the Hydrobase2 climatological monthly mean temperature data. The authors also thank Y. Li for kindly providing the original figure of surface ARGOS drifter trajectories. The authors would like to thank the associate editor, Dr. Hidenori Aiki, and the three anonymous reviewers for their valuable comments to improve this paper. NR 57 TC 5 Z9 5 U1 0 U2 7 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1616-7341 J9 OCEAN DYNAM JI Ocean Dyn. PD MAY PY 2013 VL 63 IS 5 BP 565 EP 576 DI 10.1007/s10236-013-0607-3 PG 12 WC Oceanography SC Oceanography GA 138NM UT WOS:000318515300008 ER PT J AU Bischoff, C Brizius, A Buder, I Chinone, Y Cleary, K Dumoulin, RN Kusaka, A Monsalve, R Naess, SK Newburgh, LB Nixon, G Reeves, R Smith, KM Vanderlinde, K Wehus, IK Bogdan, M Bustos, R Church, SE Davis, R Dickinson, C Eriksen, HK Gaier, T Gundersen, JO Hasegawa, M Hazumi, M Holler, C Huffenberger, KM Imbriale, WA Ishidoshiro, K Jones, ME Kangaslahti, P Kapner, DJ Lawrence, CR Leitch, EM Limon, M McMahon, JJ Miller, AD Nagai, M Nguyen, H Pearson, TJ Piccirillo, L Radford, SJE Readhead, ACS Richards, JL Samtleben, D Seiffert, M Shepherd, MC Staggs, ST Tajima, O Thompson, KL Williamson, R Winstein, B Wollack, EJ Zwart, JTL AF Bischoff, C. Brizius, A. Buder, I. Chinone, Y. Cleary, K. Dumoulin, R. N. Kusaka, A. Monsalve, R. Naess, S. K. Newburgh, L. B. Nixon, G. Reeves, R. Smith, K. M. Vanderlinde, K. Wehus, I. K. Bogdan, M. Bustos, R. Church, S. E. Davis, R. Dickinson, C. Eriksen, H. K. Gaier, T. Gundersen, J. O. Hasegawa, M. Hazumi, M. Holler, C. Huffenberger, K. M. Imbriale, W. A. Ishidoshiro, K. Jones, M. E. Kangaslahti, P. Kapner, D. J. Lawrence, C. R. Leitch, E. M. Limon, M. McMahon, J. J. Miller, A. D. Nagai, M. Nguyen, H. Pearson, T. J. Piccirillo, L. Radford, S. J. E. Readhead, A. C. S. Richards, J. L. Samtleben, D. Seiffert, M. Shepherd, M. C. Staggs, S. T. Tajima, O. Thompson, K. L. Williamson, R. Winstein, B. Wollack, E. J. Zwart, J. T. L. CA QUIET Collaboration TI THE Q/U IMAGING EXPERIMENT INSTRUMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; instrumentation: detectors; instrumentation: polarimeters; telescopes ID MICROWAVE-ANISOTROPY-PROBE; BACKGROUND POLARIZATION; WMAP OBSERVATIONS; QUIET EXPERIMENT; ANGULAR SCALE; SUBMILLIMETER; MILLIMETER; DESIGN; RADIOMETERS; POLARIMETRY AB The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(similar to 1 degrees). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 mu Ks(1/2)) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r < 0.1. The 84-element W-band polarimeter array has a sensitivity of 87 mu Ks(1/2) at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r < 0.01. The two arrays together cover multipoles in the range l similar to 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument. C1 [Bischoff, C.; Brizius, A.; Buder, I.; Kusaka, A.; Smith, K. M.; Bogdan, M.; Kapner, D. J.; Tajima, O.; Williamson, R.; Winstein, B.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bischoff, C.; Buder, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brizius, A.; Samtleben, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Chinone, Y.; Hasegawa, M.; Hazumi, M.; Ishidoshiro, K.; Nagai, M.; Tajima, O.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan. [Chinone, Y.] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Cleary, K.; Reeves, R.; Gaier, T.; Pearson, T. J.; Radford, S. J. E.; Readhead, A. C. S.; Richards, J. L.; Shepherd, M. C.; Williamson, R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Dumoulin, R. N.; Newburgh, L. B.; Limon, M.; Miller, A. D.; Williamson, R.; Zwart, J. T. L.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Dumoulin, R. N.; Newburgh, L. B.; Limon, M.; Miller, A. D.; Williamson, R.; Zwart, J. T. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kusaka, A.; Newburgh, L. B.; Nixon, G.; Smith, K. M.; Staggs, S. T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Monsalve, R.; Bustos, R.; Gundersen, J. O.; Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Monsalve, R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Naess, S. K.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Wehus, I. K.] Univ Oslo, Dept Phys, N-0316 Oslo, Norway. [Wehus, I. K.; Holler, C.; Jones, M. E.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Bustos, R.] Univ Chile, Dept Astron, Santiago, Chile. [Bustos, R.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Church, S. E.; Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Church, S. E.; Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Davis, R.; Dickinson, C.; Piccirillo, L.] Univ Manchester, Ctr Astrophys, Jodrell Bank, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Eriksen, H. K.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway. [Gaier, T.; Imbriale, W. A.; Kangaslahti, P.; Lawrence, C. R.; Leitch, E. M.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kapner, D. J.] Micro Encoder Inc, Kirkland, WA 98034 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Nguyen, H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Samtleben, D.] Nikhef, Amsterdam, Netherlands. [Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zwart, J. T. L.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. RP Bischoff, C (reprint author), Univ Chicago, Enrico Fermi Inst, Dept Phys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM newburgh@princeton.edu RI Reeves, Rodrigo/H-2812-2014; Williamson, Ross/H-1734-2015; Pearson, Timothy/N-2376-2015; Wollack, Edward/D-4467-2012; OI Reeves, Rodrigo/0000-0001-5704-271X; Williamson, Ross/0000-0002-6945-2975; Huffenberger, Kevin/0000-0001-7109-0099; Bischoff, Colin/0000-0001-9185-6514; Zwart, Jonathan/0000-0002-4967-946X; Pearson, Timothy/0000-0001-5213-6231; Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698; radford, simon/0000-0001-9113-1660 FU NSF [AST-0506648, PHY-0855887, PHY-0355328, AST-0448909, AST-1010016, PHY-0551142]; KAKENHI [20244041, 20740158, 21111002]; KIPAC Enterprise; Strategic Alliance for the Implementation of New Technologies (SAINT); Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Fermilab; Kavli Institute for Cosmological Physics; University of Chicago; JPL RTD program; STFC Advanced Fellowship; ERC IRG; CONICYT [PFB-06]; ALMA-Conicyt [31070015]; Sloan foundation; ERC; [PRODEX C90284] FX Support for the QUIET instrument and operation comes through the NSF cooperative agreement AST-0506648. Support was also provided by NSF awards PHY-0855887, PHY-0355328, AST-0448909, AST-1010016, and PHY-0551142; KAKENHI 20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise grant; and by the Strategic Alliance for the Implementation of New Technologies (SAINT). This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.; Some work was performed on the Joint Fermilab-KICP Supercomputing Cluster, supported by grants from Fermilab, the Kavli Institute for Cosmological Physics, and the University of Chicago. Some work was performed on the Titan Cluster, owned and maintained by the University of Oslo and NOTUR (the Norwegian High Performance Computing Consortium), and on the Central Computing System, owned and operated by the Computing Research Center at KEK. Portions of this work were performed at the Jet Propulsion Laboratory (JPL) and California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration. The Q-band modules were developed using funding from the JPL R&TD program. We acknowledge the Northrop Grumman Corporation for collaboration in the development and fabrication of HEMT-based cryogenic temperature-compatible MMICs.; C.D. acknowledges an STFC Advanced Fellowship and an ERC IRG grant under FP7. R. B. acknowledges support from CONICYT project Basal PFB-06 and ALMA-Conicyt 31070015. A. D. M. acknowledges a Sloan foundation fellowship. H. K. E. acknowledges an ERC Starting Grant under FP7. NR 54 TC 14 Z9 14 U1 1 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 MAY 1 PY 2013 VL 768 IS 1 AR 9 DI 10.1088/0004-637X/768/1/9 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500009 ER PT J AU Daly, AM Bermudez, C Lopez, A Tercero, B Pearson, JC Marcelino, N Alonso, JL Cernicharo, J AF Daly, A. M. Bermudez, C. Lopez, A. Tercero, B. Pearson, J. C. Marcelino, N. Alonso, J. L. Cernicharo, J. TI LABORATORY CHARACTERIZATION AND ASTROPHYSICAL DETECTION OF VIBRATIONALLY EXCITED STATES OF ETHYL CYANIDE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual objects (Orion KL); ISM: molecules; line: identification; surveys ID MILLIMETER-WAVE OBSERVATIONS; MOLECULAR LINE SURVEY; ROTATIONAL SPECTRUM; ORION-KL; PROPIONITRILE C2H5CN; MICROWAVE-SPECTRUM; APERTURE SYNTHESIS; METHYL FORMATE; GHZ; ABUNDANCES AB Ethyl cyanide, CH3CH2CN, is an important interstellar molecule with a very dense rotational-vibrational spectrum. On the basis of new laboratory data in the range of 17-605 GHz and ab initio calculations, two new vibrational states, nu(12) and nu(20), have been detected in molecular clouds of Orion. Laboratory data consist of Stark spectroscopy (17-110 GHz) and frequency-modulated spectrometers (GEM laboratory in Valladolid: 17-170, 270-360 GHz; Toyama: 26-200 GHz; Emory: 200-240 GHz; Ohio State: 258-368 GHz; and JPL: 270-318, 395-605 GHz). More than 700 distinct lines of each species were measured in J up to 71 and in K-a up to 25. The states were fitted with Watson's S-reduction Hamiltonian. The two new states have been identified in the interstellar medium toward the Orion Nebula (Orion KL). The ground state, the isotopologues of CH3CH2CN, and the vibrationally excited states have been fitted to obtain column densities and to derive vibrational temperatures. All together, ethyl cyanide is responsible for more than 2000 lines in the observed frequency range of 80-280 GHz. C1 [Daly, A. M.; Bermudez, C.; Alonso, J. L.] Univ Valladolid, Area Quim Fis, Labs Espect & Bioespect, Unidad Asociada CSIC,GEM, E-47005 Valladolid, Spain. [Lopez, A.; Tercero, B.; Cernicharo, J.] INTA CSIC, CAB, Dept Astrophys, E-28850 Madrid, Spain. [Pearson, J. C.] CALTECH, Jet Prop Lab, Padadena, CA 91109 USA. [Marcelino, N.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Daly, AM (reprint author), Univ Valladolid, Area Quim Fis, Labs Espect & Bioespect, Unidad Asociada CSIC,GEM, Edificio Quifima, E-47005 Valladolid, Spain. EM adammichael.daly@uva.es; cbermu@qf.uva.es; lopezja@cab.inta-csic.es; terceromb@cab.inta-csic.es; John.C.Pearson@jpl.nasa.gov; nmarceli@nrao.edu; jlalonso@qf.uva.es; jcernicharo@cab.inta-csic.es FU Spanish MICINN [AYA2006-14786, AYA2009-07304, BES-2011-047695, CTQ2010-19008]; CONSOLIDER program "ASTROMOL" [CSD2009-00038]; NASA; NASA Astrophysics Research and Analysis program FX A.L., J.C., and B. T. thank Spanish MICINN for support under grants AYA2006-14786 and AYA2009-07304. C. B., A. M. D., and J.L.A. thank the Spanish MICINN for the FPI grant (BES-2011-047695) associated with the CTQ2010-19008 project. The Spanish authors also thank the CONSOLIDER program "ASTROMOL" CSD2009-00038 for support. A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. J.C. P. thanks the NASA Astrophysics Research and Analysis program for support. NR 55 TC 21 Z9 21 U1 2 U2 21 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 MAY 1 PY 2013 VL 768 IS 1 AR 81 DI 10.1088/0004-637X/768/1/81 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500081 ER PT J AU Gatuzz, E Garcia, J Mendoza, C Kallman, TR Witthoeft, M Lohfink, A Bautista, MA Palmeri, P Quinet, P AF Gatuzz, E. Garcia, J. Mendoza, C. Kallman, T. R. Witthoeft, M. Lohfink, A. Bautista, M. A. Palmeri, P. Quinet, P. TI PHOTOIONIZATION MODELING OF OXYGEN K ABSORPTION IN THE INTERSTELLAR MEDIUM: THE CHANDRA GRATING SPECTRA OF XTE J1817-330 SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; ISM: general; stars: individual (XTE J1817-330); X-rays: binaries; X-rays: general ID X-RAY SPECTROSCOPY; XMM-NEWTON OBSERVATION; ATOMIC DATA; SHELL PHOTOABSORPTION; OPACITY CALCULATIONS; LINES; IONS; GALAXY; DECAY; IRON AB We present detailed analyses of oxygen K absorption in the interstellar medium (ISM) using four high-resolution Chandra spectra toward the X-ray low-mass binary XTE J1817-330. The 11-25 angstrom broadband is described with a simple absorption model that takes into account the pile-up effect and results in an estimate of the hydrogen column density. The oxygen K-edge region (21-25 angstrom) is fitted with the physical warmabs model, which is based on a photoionization model grid generated with the xstar code with the most up-to-date atomic database. This approach allows a benchmark of the atomic data which involves wavelength shifts of both the K lines and photoionization cross sections in order to fit the observed spectra accurately. As a result we obtain a column density of N-H = 1.38 +/- 0.01 x 10(21) cm(-2); an ionization parameter of log xi = -2.70 +/- 0.023; an oxygen abundance of A(O) = 0.689(-0.010)(+0.015); and ionization fractions of OI/O = 0.911, OII/O = 0.077, and OIII/O = 0.012 that are in good agreement with results from previous studies. Since the oxygen abundance in warmabs is given relative to the solar standard of Grevesse & Sauval, a rescaling with the revision by Asplund et al. yields A(O) = 0.952(-0.013)(+0.020), a value close to solar that reinforces the new standard. We identify several atomic absorption lines-K alpha, K beta, and K gamma in OI and OII and K alpha in OIII, OvI, and OvII-the last two probably residing in the neighborhood of the source rather than in the ISM. This is the first firm detection of oxygen K resonances with principal quantum numbers n > 2 associated with ISM cold absorption. C1 [Gatuzz, E.; Mendoza, C.] IVIC, Ctr Fis, Miranda, Venezuela. [Garcia, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Garcia, J.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA. [Garcia, J.; Kallman, T. R.; Witthoeft, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mendoza, C.] Univ Los Andes CeCalCULA, Corporaci Parque Tecnol Merida, Centro Nacl Calculo Cient, Merida 5101, Venezuela. [Bautista, M. A.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Palmeri, P.; Quinet, P.] Univ Mons UMONS, B-7000 Mons, Belgium. [Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium. RP Gatuzz, E (reprint author), IVIC, Ctr Fis, POB 20632,Caracas 1020A, Miranda, Venezuela. EM egatuzz@ivic.gob.ve; javier@astro.umd.edu; timothy.r.kallman@nasa.gov; michael.c.witthoeft@nasa.gov; alohfink@astro.umd.edu; manuel.bautista@wmich.edu; palmeri@umons.ac.be; quinet@umons.ac.be FU COSPAR Fellowship Program FX Part of this work was carried out by Efrain Gatuzz during attendance of the Committee On Space Research (COSPAR) Capacity Building Workshop in San Juan, Argentina in 2011 July, and visits in 2011 August to the Laboratory of High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA, and in 2012 February-March to the European Space Astronomy Centre (ESAC), Madrid, Spain, the latter funded by the COSPAR Fellowship Program. Warm hospitality and tutelage at these institutions are kindly acknowledged, in particular, from Andy Pollock and Carlos Gabriel at ESAC. We also thank Michael Nowak from MIT for useful discussions relating to the pile-up model and ISIS implementation. NR 54 TC 16 Z9 16 U1 2 U2 6 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 MAY 1 PY 2013 VL 768 IS 1 AR 60 DI 10.1088/0004-637X/768/1/60 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500060 ER PT J AU Hanish, DJ Teplitz, HI Capak, P Desai, V Armus, L Brinkworth, C Brooke, T Colbert, J Fadda, D Frayer, D Huynh, M Lacy, M Murphy, E Noriega-Crespo, A Paladini, R Scarlata, C Shenoy, S AF Hanish, D. J. Teplitz, H. I. Capak, P. Desai, V. Armus, L. Brinkworth, C. Brooke, T. Colbert, J. Fadda, D. Frayer, D. Huynh, M. Lacy, M. Murphy, E. Noriega-Crespo, A. Paladini, R. Scarlata, C. Shenoy, S. CA SAFIRES Team TI FAR-INFRARED PROPERTIES OF TYPE 1 QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; quasars: general; surveys ID SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; 7TH DATA RELEASE; SOURCE EXTRACTION; SPITZER; STARBURSTS; SELECTION; DENSITY; ATLAS AB We use the Spitzer Space Telescope Enhanced Imaging Products and the Spitzer Archival Far-InfraRed Extragalactic Survey to study the spectral energy distributions (SEDs) of spectroscopically confirmed type 1 quasars selected from the Sloan Digital Sky Survey (SDSS). By combining the Spitzer and SDSS data with the Two Micron All Sky Survey, we are able to construct a statistically robust rest-frame 0.1-100 mu m type 1 quasar template. We find that the quasar population is well-described by a single power-law SED at wavelengths less than 20 mu m, in good agreement with previous work. However, at longer wavelengths, we find a significant excess in infrared luminosity above an extrapolated power-law, along with significant object-to-object dispersion in the SED. The mean excess reaches a maximum of 0.8 dex at rest-frame wavelengths near 100 mu m. C1 [Hanish, D. J.; Teplitz, H. I.; Capak, P.; Desai, V.; Armus, L.; Brinkworth, C.; Brooke, T.; Colbert, J.; Fadda, D.; Noriega-Crespo, A.; Paladini, R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Huynh, M.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Lacy, M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Murphy, E.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Scarlata, C.] Univ Minnesota, Minnesota Inst Astrophys, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Shenoy, S.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Hanish, DJ (reprint author), CALTECH, Spitzer Sci Ctr, MC 220-6,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM hanish@ipac.caltech.edu FU NASA [NASA-ADAP NNX10AD52G]; NASA; NSF; Alfred P. Sloan Foundation FX Support for this work was provided by NASA through contract NASA-ADAP NNX10AD52G. This publication makes use of (1) raw data from the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory/California Institute of Technology under NASA contract, (2) data products from the Two Micron All Sky Survey, a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF, and (3) the SDSS, managed by the Astrophysical Research Consortium for the Participating Institutions and funded by the Alfred P. Sloan Foundation, the Participating Institutions, and many others. NR 28 TC 3 Z9 3 U1 0 U2 2 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 MAY 1 PY 2013 VL 768 IS 1 AR 13 DI 10.1088/0004-637X/768/1/13 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500013 ER PT J AU Huppenkothen, D Watts, AL Uttley, P van der Horst, AJ van der Klis, M Kouveliotou, C Gogus, E Granot, J Vaughan, S Finger, MH AF Huppenkothen, Daniela Watts, Anna L. Uttley, Phil van der Horst, Alexander J. van der Klis, Michiel Kouveliotou, Chryssa Gogus, Ersin Granot, Jonathan Vaughan, Simon Finger, Mark H. TI QUASI-PERIODIC OSCILLATIONS AND BROADBAND VARIABILITY IN SHORT MAGNETAR BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; pulsars: individual (SGR 0501+4516); stars: magnetic field; stars: neutron; X-rays: bursts ID X-RAY OSCILLATIONS; POWER-DENSITY SPECTRUM; REPEATER GIANT FLARES; SOFT GAMMA-REPEATERS; NEUTRON-STAR; SGR 1806-20; STATISTICAL PROPERTIES; 2004 HYPERFLARE; DISCOVERY; EMISSION AB The discovery of quasi-periodic oscillations (QPOs) in magnetar giant flares has opened up prospects for neutron star asteroseismology. However, with only three giant flares ever recorded, and only two with data of sufficient quality to search for QPOs, such analysis is seriously data limited. We set out a procedure for doing QPO searches in the far more numerous, short, less energetic magnetar bursts. The short, transient nature of these bursts requires the implementation of sophisticated statistical techniques to make reliable inferences. Using Bayesian statistics, we model the periodogram as a combination of red noise at low frequencies and white noise at high frequencies, which we show is a conservative approach to the problem. We use empirical models to make inferences about the potential signature of periodic and QPOs at these frequencies. We compare our method with previously used techniques and find that although it is on the whole more conservative, it is also more reliable in ruling out false positives. We illustrate our Bayesian method by applying it to a sample of 27 bursts from the magnetar SGR J0501+4516 observed by the Fermi Gamma-ray Burst Monitor, and we find no evidence for the presence of QPOs in any of the bursts in the unbinned spectra, but do find a candidate detection in the binned spectra of one burst. However, whether this signal is due to a genuine quasi-periodic process, or can be attributed to unmodeled effects in the noise is at this point a matter of interpretation. C1 [Huppenkothen, Daniela; Watts, Anna L.; Uttley, Phil; van der Horst, Alexander J.; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Off Sci & Technol, ZP12, Huntsville, AL 35812 USA. [Gogus, Ersin] Sabanci Univ, TR-34956 Istanbul, Turkey. [Granot, Jonathan] Open Univ Israel, IL-43537 Raanana, Israel. [Vaughan, Simon] Univ Leicester, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. [Finger, Mark H.] Univ Space Res Assoc, Huntsville, AL 35805 USA. RP Huppenkothen, D (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands. EM D.Huppenkothen@uva.nl FU Netherlands Organization for Scientific Research (NWO); NASA [NNH07ZDA001-GLAST]; Scientific and Technological Research Council of Turkey (TUBITAK) [109T755] FX D.H. and A. L. W. acknowledge support from a Netherlands Organization for Scientific Research (NWO) Vidi Fellowship (PI: A. Watts), and would like to thank Jason Farquhar for useful discussions. C. K. was partially supported by NASA grant NNH07ZDA001-GLAST. E. G. acknowledges support from the Scientific and Technological Research Council of Turkey (TUBITAK) through grant 109T755. NR 70 TC 17 Z9 17 U1 1 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 MAY 1 PY 2013 VL 768 IS 1 AR 87 DI 10.1088/0004-637X/768/1/87 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500087 ER PT J AU Kajisawa, M Shioya, Y Aida, Y Ideue, Y Taniguchi, Y Nagao, T Murayama, T Matsubayashi, K Riguccini, L AF Kajisawa, M. Shioya, Y. Aida, Y. Ideue, Y. Taniguchi, Y. Nagao, T. Murayama, T. Matsubayashi, K. Riguccini, L. TI ENVIRONMENTAL EFFECTS ON STAR FORMATION ACTIVITY AT z similar to 0.9 IN THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: star formation ID SQUARE DEGREE FIELD; FORMATION-DENSITY RELATION; ALPHA LUMINOSITY FUNCTION; EVOLUTION SURVEY COSMOS; DIGITAL SKY SURVEY; SUBARU DEEP FIELD; STELLAR MASS; H-ALPHA; FORMATION HISTORY; FORMING GALAXIES AB We investigated the fraction of [OII] emitters in galaxies at z similar to 0.9 as a function of the local galaxy density in the Hubble Space Telescope (HST) COSMOS 2 deg(2) field. [OII] emitters are selected by the narrowband excess technique with the NB711-band imaging data taken with Suprime-Cam on the Subaru telescope. We carefully selected 614 photo-z-selected galaxies with M-U3500 < -19.31 at z = 0.901 - 0.920, which includes 195 [OII] emitters, to directly compare the results with our previous study at z similar to 1.2. We found that the fraction is almost constant at 0.3 Mpc (2) < Sigma(10th) < 10 Mpc (2). We also checked the fraction of galaxies with blue rest-frame colors of NUV - R < 2 in our photo-z-selected sample, and found that the fraction of blue galaxies does not significantly depend on the local density. On the other hand, the semi-analytic model of galaxy formation predicted that the fraction of star-forming galaxies at z similar to 0.9 decreases with increasing projected galaxy density even if the effects of the projection and the photo-z error in our analysis were taken into account. The fraction of [OII] emitters decreases from similar to 60% at z similar to 1.2 to similar to 30% at z similar to 0.9 independent of galaxy environment. The decrease of the [OII] emitter fraction could be explained mainly by the rapid decrease of star formation activity in the universe from z similar to 1.2 to z similar to 0.9. C1 [Kajisawa, M.; Shioya, Y.; Taniguchi, Y.; Nagao, T.; Matsubayashi, K.; Riguccini, L.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Kajisawa, M.; Aida, Y.; Ideue, Y.] Ehime Univ, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan. [Nagao, T.] Kyoto Univ, Hakubi Project, Sakyo Ku, Kyoto 6068302, Japan. [Nagao, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Murayama, T.] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Riguccini, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kajisawa, M (reprint author), Ehime Univ, Res Ctr Space & Cosm Evolut, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. EM kajisawa@cosmos.phys.sci.ehime-u.ac.jp FU NASA [HST-GO-09822, NAS 5-26555, 1407]; Japan Society for the Promotion of Science [17253001, 19340046, 23244031, 23654068, 23740152]; ESA Member States; European Southern Observatory, Chile [175.A-0839] FX We thank the referee for invaluable suggestions and comments. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We greatly acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. This work was financially supported in part by the Japan Society for the Promotion of Science (Nos. 17253001, 19340046, 23244031, 23654068, and 23740152).; Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc, under NASA contract NAS 5-26555. Also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; and the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France, TERAPIX, and the University of Hawaii. NR 47 TC 1 Z9 1 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 51 DI 10.1088/0004-637X/768/1/51 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500051 ER PT J AU Kraus, S Ireland, MJ Sitko, ML Monnier, JD Calvet, N Espaillat, C Grady, CA Harries, TJ Honig, SF Russell, RW Swearingen, JR Werren, C Wilner, DJ AF Kraus, Stefan Ireland, Michael J. Sitko, Michael L. Monnier, John D. Calvet, Nuria Espaillat, Catherine Grady, Carol A. Harries, Tim J. Hoenig, Sebastian F. Russell, Ray W. Swearingen, Jeremy R. Werren, Chelsea Wilner, David J. TI RESOLVING THE GAP AND AU-SCALE ASYMMETRIES IN THE PRE-TRANSITIONAL DISK OF V1247 ORIONIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; protoplanetary disks; stars: pre-main sequence; techniques: interferometric ID PRE-MAIN-SEQUENCE; YOUNG STELLAR OBJECTS; STAR SAO 206462; ALL-SKY SURVEY; T TAURI STARS; PROTOPLANETARY DISKS; INNER DISK; INFRARED VARIABILITY; TRANSITIONAL DISKS; DATA REDUCTION AB Pre-transitional disks are protoplanetary disks with a gapped disk structure, potentially indicating the presence of young planets in these systems. In order to explore the structure of these objects and their gap-opening mechanism, we observed the pre-transitional disk V1247 Orionis using the Very Large Telescope Interferometer, the Keck Interferometer, Keck-II, Gemini South, and IRTF. This allows us to spatially resolve the AU-scale disk structure from near-to mid-infrared wavelengths (1.5-13 mu m), tracing material at different temperatures and over a wide range of stellocentric radii. Our observations reveal a narrow, optically thick inner-disk component (located at 0.18 AU from the star) that is separated from the optically thick outer disk (radii greater than or similar to 46 AU), providing unambiguous evidence for the existence of a gap in this pre-transitional disk. Surprisingly, we find that the gap region is filled with significant amounts of optically thin material with a carbon-dominated dust mineralogy. The presence of this optically thin gap material cannot be deduced solely from the spectral energy distribution, yet it is the dominant contributor at mid-infrared wavelengths. Furthermore, using Keck/NIRC2 aperture masking observations in the H, K', and L' bands, we detect asymmetries in the brightness distribution on scales of similar to 15-40 AU, i.e., within the gap region. The detected asymmetries are highly significant, yet their amplitude and direction changes with wavelength, which is not consistent with a companion interpretation but indicates an inhomogeneous distribution of the gap material. We interpret this as strong evidence for the presence of complex density structures, possibly reflecting the dynamical interaction of the disk material with sub-stellar mass bodies that are responsible for the gap clearing. C1 [Kraus, Stefan; Espaillat, Catherine; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kraus, Stefan; Monnier, John D.; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Kraus, Stefan; Harries, Tim J.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Ireland, Michael J.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Sitko, Michael L.; Swearingen, Jeremy R.; Werren, Chelsea] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Sitko, Michael L.] Space Sci Inst, Boulder, CO 80301 USA. [Grady, Carol A.] Eureka Sci Inc, Oakland, CA 94602 USA. [Grady, Carol A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Hoenig, Sebastian F.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Russell, Ray W.] Aerosp Corp, Los Angeles, CA 90009 USA. RP Kraus, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA. OI Hoenig, Sebastian/0000-0002-6353-1111 FU Keck observatory (NASA program) [N121IV]; Keck observatory (NOAO program) [N121N2]; Gemini South (NOAO program) [GS-2011B-Q-19]; ESO telescopes at the Paranal Observatory [088.C-0868(A), 088.C-0763(A+B)]; National Aeronautics and Space Administration; California Institute of Technology (Caltech); NASA through the Sagan Fellowship Program; W. M. Keck Foundation; Aerospace Corporation's Independent Research and Development (IRD) program; NASA ADP grant [NNX09AC73G] FX Based on observations made with the Keck observatory (NASA program ID N121IV and NOAO program ID N121N2), Gemini South (NOAO program ID GS-2011B-Q-19), and with ESO telescopes at the Paranal Observatory (ESO program IDs 088.C-0868(A)and 088.C-0763(A+B)).; Visiting Astronomer, NASA Infrared Telescope Facility, operated by the University of Hawaii under contract with the National Aeronautics and Space Administration.; We thank the referee, Jose Caballero, for his detailed report, which helped to improve the presentation of this paper. This work was done in part under contract with the California Institute of Technology (Caltech), funded by NASA through the Sagan Fellowship Program (S. K. and C. E. are Sagan Fellows). Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work was supported in part by the Aerospace Corporation's Independent Research and Development (IR&D) program. This work was supported by NASA ADP grant NNX09AC73G. NR 87 TC 19 Z9 19 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 80 DI 10.1088/0004-637X/768/1/80 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500080 ER PT J AU Martini, P Miller, ED Brodwin, M Stanford, SA Gonzalez, AH Bautz, M Hickox, RC Stern, D Eisenhardt, PR Galametz, A Norman, D Jannuzi, BT Dey, A Murray, S Jones, C Brown, MJI AF Martini, Paul Miller, E. D. Brodwin, M. Stanford, S. A. Gonzalez, Anthony H. Bautz, M. Hickox, R. C. Stern, D. Eisenhardt, P. R. Galametz, A. Norman, D. Jannuzi, B. T. Dey, A. Murray, S. Jones, C. Brown, M. J. I. TI THE CLUSTER AND FIELD GALAXY ACTIVE GALACTIC NUCLEUS FRACTION AT z=1-1.5: EVIDENCE FOR A REVERSAL OF THE LOCAL ANTICORRELATION BETWEEN ENVIRONMENT AND AGN FRACTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: evolution; X-rays: galaxies; X-rays: galaxies: clusters; X-rays: general ID SUPERMASSIVE BLACK-HOLES; DIGITAL-SKY-SURVEY; IRAC SHALLOW SURVEY; SIMILAR-TO 1; CHANDRA MULTIWAVELENGTH PROJECT; ULTRALUMINOUS INFRARED GALAXIES; FORMATION-DENSITY RELATION; EMISSION-LINE GALAXIES; HUBBLE-SPACE-TELESCOPE; LOW-REDSHIFT CLUSTERS AB The fraction of cluster galaxies that host luminous active galactic nuclei (AGNs) is an important probe of AGN fueling processes, the cold interstellar medium at the centers of galaxies, and how tightly black holes and galaxies co-evolve. We present a new measurement of the AGN fraction in a sample of 13 clusters of galaxies (M >= 10(14) M-circle dot) at 1 < z < 1.5 selected from the Spitzer/IRAC Shallow Cluster Survey, as well as the field fraction in the immediate vicinity of these clusters, and combine these data with measurements from the literature to quantify the relative evolution of cluster and field AGN from the present to z similar to 3. We estimate that the cluster AGN fraction at 1 < z < 1.5 is f(A) = 3.0(-1.4)(+2.4)% for AGNs with a rest-frame, hard X-ray luminosity greater than L-X,L- H >= 10(44) erg s(-1). This fraction is measured relative to all cluster galaxies more luminous than M-3.6*(z)+ 1, where M-3.6*(z) is the absolute magnitude of the break in the galaxy luminosity function at the cluster redshift in the IRAC 3.6 mu m bandpass. The cluster AGN fraction is 30 times greater than the 3 sigma upper limit on the value for AGNs of similar luminosity at z similar to 0.25, as well as more than an order of magnitude greater than the AGN fraction at z similar to 0.75. AGNs with L-X,L- H >= 10(43) erg s(-1) exhibit similarly pronounced evolution with redshift. In contrast to the local universe, where the luminous AGN fraction is higher in the field than in clusters, the X-ray and MIR-selected AGN fractions in the field and clusters are consistent at 1 < z < 1.5. This is evidence that the cluster AGN population has evolved more rapidly than the field population from z similar to 1.5 to the present. This environment-dependent AGN evolution mimics the more rapid evolution of star-forming galaxies in clusters relative to the field. C1 [Martini, Paul] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Martini, Paul] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Miller, E. D.; Bautz, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Stern, D.; Eisenhardt, P. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Norman, D.; Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Jannuzi, B. T.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Jannuzi, B. T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murray, S.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. RP Martini, P (reprint author), North Amer ALMA Sci Ctr, Charlottesville, VA 22903 USA. EM martini@astronomy.ohio-state.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 FU U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; National Aeronautics and Space Administration through Chandra Award [GO9-0150A]; National Aeronautics Space Administration [NAS8-03060] FX We thank Daryl Haggard for calculating the field AGN fraction based on our AGN and galaxy luminosity thresholds. We also appreciate a thoughtful and helpful review from the referee. P. M. appreciates support from the sabbatical visitor program at the North American ALMA Science Center (NAASC) at NRAO and the hospitality of both the NAASC and the University of Virginia while this work was completed. The work of P. R. M. E. and D. S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO9-0150A issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. NR 117 TC 37 Z9 38 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 MAY 1 PY 2013 VL 768 IS 1 AR 1 DI 10.1088/0004-637X/768/1/1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500001 ER PT J AU Mathews, WG Temi, P Brighenti, F Amblard, A AF Mathews, William G. Temi, Pasquale Brighenti, Fabrizio Amblard, Alexandre TI VARIATIONS OF MID- AND FAR-INFRARED LUMINOSITIES AMONG EARLY-TYPE GALAXIES: RELATION TO STELLAR METALLICITY AND COLD DUST SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: ISM; infrared: galaxies; infrared: ISM ID FORMATION RATE INDICATORS; GIANT BRANCH STARS; ELLIPTIC GALAXIES; SPITZER OBSERVATIONS; POPULATION HISTORIES; GRADIENTS; CORES; GAS; CALIBRATION; PARAMETERS AB The Hubble morphological sequence from early to late galaxies corresponds to an increasing rate of specific star formation. The Hubble sequence also follows a banana-shaped correlation between 24 and 70 mu m luminosities, both normalized with the K-band luminosity. We show that this correlation is significantly tightened if galaxies with central active galactic nucleus (AGN) emission are removed, but the cosmic scatter of elliptical galaxies in both 24 and 70 mu m luminosities remains significant along the correlation. We find that the 24 mu m variation among ellipticals correlates with stellar metallicity, reflecting emission from hot dust in winds from asymptotic giant branch stars of varying metallicity. Infrared surface brightness variations in elliptical galaxies indicate that the K - 24 color profile is U-shaped for reasons that are unclear. In some elliptical galaxies, cold interstellar dust emitting at 70 and 160 mu m may arise from recent gas-rich mergers. However, we argue that most of the large range of 70 mu m luminosity in elliptical galaxies is due to dust transported from galactic cores by feedback events in (currently IR-quiet) AGNs. Cooler dusty gas naturally accumulates in the cores of elliptical galaxies due to dust-cooled local stellar mass loss and may accrete onto the central black hole, releasing energy. AGN-heated gas can transport dust in cores 5-10 kpc out into the hot gas atmospheres where it radiates extended 70 mu m emission but is eventually destroyed by sputtering. This, and some modest star formation, defines a cycle of dust creation and destruction. Elliptical galaxies evidently undergo large transient excursions in the banana plot in times comparable to the sputtering time or AGN duty cycle, 10 Myr. Normally regarded as passive, elliptical galaxies are the most active galaxies in the IR color-color correlation. C1 [Mathews, William G.; Brighenti, Fabrizio] Univ Calif Santa Cruz, Lick Observ, Board Studies Astron & Astrophys, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Temi, Pasquale; Amblard, Alexandre] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Brighenti, Fabrizio] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. RP Mathews, WG (reprint author), Univ Calif Santa Cruz, Lick Observ, Board Studies Astron & Astrophys, Univ Calif Observ, Santa Cruz, CA 95064 USA. EM mathews@ucolick.org; pasquale.temi@nasa.gov; fabrizio.brighenti@unibo.it RI amblard, alexandre/L-7694-2014 OI amblard, alexandre/0000-0002-2212-5395 FU NASA [1407]; NSF; NASA ADP; PRIN MIUR [2010LY5N2T] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Studies of the evolution of hot gas in elliptical galaxies at UC Santa Cruz are supported by an NSF grant for which we are very grateful. Support for this work was provided by the NASA ADP Grant. F.B. acknowledges financial support from PRIN MIUR 2010-2011, prot. 2010LY5N2T. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr) and the NASA/IPAC Extragalactic Database (NED). NR 36 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 28 DI 10.1088/0004-637X/768/1/28 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500028 ER PT J AU Ofek, EO Lin, L Kouveliotou, C Younes, G Gogus, E Kasliwal, MM Cao, Y AF Ofek, E. O. Lin, L. Kouveliotou, C. Younes, G. Gogus, E. Kasliwal, M. M. Cao, Y. TI SN 2009ip: CONSTRAINTS ON THE PROGENITOR MASS-LOSS RATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: mass-loss; supernovae: general; supernovae: individual (SN 2009ip) ID RICH CIRCUMSTELLAR MEDIUM; X-RAY-EMISSION; SHOCK BREAKOUT; LUMINOUS SUPERNOVA; IIN SUPERNOVAE; STAR; WIND; ABSORPTION; RADIO; SWIFT AB Some supernovae (SNe) show evidence for mass-loss events taking place prior to their explosions. Measuring their pre-outburst mass-loss rates provides essential information regarding the mechanisms that are responsible for these events. Here we present XMM-Newton and Swift X-ray observations taken after the latest, and presumably the final, outburst of SN 2009ip. We use these observations as well as new near-infrared and visible-light spectra and published radio and visible-light observations to put six independent order-of-magnitude constraints on the mass-loss rate of the SN progenitor prior to the explosion. Our methods utilize the X-ray luminosity, the bound-free absorption, the H alpha luminosity, the SN rise time, free-free absorption, and the bolometric luminosity of the outburst detected prior to the explosion. Assuming spherical mass loss with a wind-density profile, we estimate that the effective mass-loss rate from the progenitor was between 10(-3) and 10(-2) M-circle dot yr(-1), over a few years prior to the explosion, with a velocity of similar to 10(3) km s(-1). This mass-loss rate corresponds to a total circumstellar matter (CSM) mass of similar to 0.04 M-circle dot, within 6 x 10(15) cm of the SN. We note that the mass-loss rate estimate based on the H alpha luminosity is higher by an order of magnitude. This can be explained if the narrow-line H alpha component is generated at radii larger than the shock radius, or if the CSM has an aspherical geometry. We discuss simple geometries which are consistent with our results. C1 [Ofek, E. O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Ofek, E. O.] Weizmann Inst Sci, Helen Kimmel Ctr Planetary Sci, IL-76100 Rehovot, Israel. [Lin, L.; Gogus, E.] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Younes, G.] Univ Space Res Assoc, Huntsville, AL 35806 USA. [Kasliwal, M. M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Cao, Y.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Ofek, EO (reprint author), Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. FU Israeli Ministry of Science; Hubble Fellowship; Carnegie-Princeton Fellowship FX We thank Orly Gnat, Udi Nakar, Stan Woosley, Nir Sapir, and Avishay Gal-Yam for productive discussions, and an anonymous referee for useful suggestions. We gratefully acknowledge the collaboration of the XMM Project team, and in particular Dr. Norbert Schartel, for the XMM ToO observations. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. NR 68 TC 25 Z9 25 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 MAY 1 PY 2013 VL 768 IS 1 AR 47 DI 10.1088/0004-637X/768/1/47 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500047 ER PT J AU Oppenheimer, BR Baranec, C Beichman, C Brenner, D Burruss, R Cady, E Crepp, JR Dekany, R Fergus, R Hale, D Hillenbrand, L Hinkley, S Hogg, DW King, D Ligon, ER Lockhart, T Nilsson, R Parry, IR Pueyo, L Rice, E Roberts, JE Roberts, LC Shao, M Sivaramakrishnan, A Soummer, R Truong, T Vasisht, G Veicht, A Vescelus, F Wallace, JK Zhai, C Zimmerman, N AF Oppenheimer, B. R. Baranec, C. Beichman, C. Brenner, D. Burruss, R. Cady, E. Crepp, J. R. Dekany, R. Fergus, R. Hale, D. Hillenbrand, L. Hinkley, S. Hogg, David W. King, D. Ligon, E. R. Lockhart, T. Nilsson, R. Parry, I. R. Pueyo, L. Rice, E. Roberts, J. E. Roberts, L. C., Jr. Shao, M. Sivaramakrishnan, A. Soummer, R. Truong, T. Vasisht, G. Veicht, A. Vescelus, F. Wallace, J. K. Zhai, C. Zimmerman, N. TI RECONNAISSANCE OF THE HR 8799 EXOSOLAR SYSTEM. I. NEAR-INFRARED SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: adaptive optics; instrumentation: spectrographs; methods: data analysis; planetary systems; stars: individual (HR 8799); techniques: spectroscopic ID INTEGRAL FIELD SPECTROGRAPH; EXTRASOLAR GIANT PLANETS; PUPIL LYOT CORONAGRAPHS; GAMMA DORADUS STARS; BROWN DWARFS; DEBRIS DISKS; MU-M; YOUNG STARS; M-BAND; COMPANIONS AB We obtained spectra in the wavelength range lambda = 995-1769 nm of all four known planets orbiting the star HR 8799. Using the suite of instrumentation known as Project 1640 on the Palomar 5 m Hale Telescope, we acquired data at two epochs. This allowed for multiple imaging detections of the companions and multiple extractions of low-resolution (R similar to 35) spectra. Data reduction employed two different methods of speckle suppression and spectrum extraction, both yielding results that agree. The spectra do not directly correspond to those of any known objects, although similarities with L and T dwarfs are present, as well as some characteristics similar to planets such as Saturn. We tentatively identify the presence of CH4 along with NH3 and/or C2H2, and possibly CO2 or HCN in varying amounts in each component of the system. Other studies suggested red colors for these faint companions, and our data confirm those observations. Cloudy models, based on previous photometric observations, may provide the best explanation for the new data presented here. Notable in our data is that these presumably co-eval objects of similar luminosity have significantly different spectra; the diversity of planets may be greater than previously thought. The techniques and methods employed in this paper represent a new capability to observe and rapidly characterize exoplanetary systems in a routine manner over a broad range of planet masses and separations. These are the first simultaneous spectroscopic observations of multiple planets in a planetary system other than our own. C1 [Oppenheimer, B. R.; Beichman, C.; Brenner, D.; Nilsson, R.; Parry, I. R.; Rice, E.; Sivaramakrishnan, A.; Soummer, R.; Veicht, A.; Zimmerman, N.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Baranec, C.; Dekany, R.; Hale, D.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Beichman, C.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Burruss, R.; Cady, E.; Ligon, E. R.; Lockhart, T.; Roberts, J. E.; Roberts, L. C., Jr.; Shao, M.; Truong, T.; Vasisht, G.; Vescelus, F.; Wallace, J. K.; Zhai, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Crepp, J. R.; Hillenbrand, L.; Hinkley, S.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Fergus, R.] NYU, Courant Inst Math, Dept Comp Sci, New York, NY 10003 USA. [Hogg, David W.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [King, D.; Parry, I. R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Pueyo, L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rice, E.] CUNY Coll Staten Isl, Dept Engn Sci & Phys, Staten Isl, NY 10314 USA. [Sivaramakrishnan, A.; Soummer, R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Oppenheimer, BR (reprint author), Amer Museum Nat Hist, Dept Astrophys, Cent Pk West & 79th St, New York, NY 10024 USA. EM bro@amnh.org RI Rice, Emily/G-4446-2013; OI Rice, Emily/0000-0002-3252-5886; Zimmerman, Neil/0000-0001-5484-1516; Hogg, David/0000-0003-2866-9403 FU National Science Foundation [AST-0215793, 0334916, 0520822, 0619922, 0804417, 0908497, 1039790, IIS-1124794]; EAGER grant [1245018]; NASA Origins of the Solar System grant [NMO7100830/102190]; NASA APRA grant [08-APRA08-0117]; NASA through American Astronomical Society's Small Research Grant Program; Helge Ax:son Johnson's foundation; NASA through Sagan Fellowship Program; National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship [AST-1203023] FX We are especially grateful for our two referees, both of whom were particularly meticulous, thorough, and fair. Their reports resulted in significant improvements in the paper. A portion of this work is or was supported by the National Science Foundation under award Nos. AST-0215793, 0334916, 0520822, 0619922, 0804417, 0908497, 1039790 and EAGER grant 1245018. A portion of the research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and was funded by internal Research and Technology Development funds. A portion of this work was supported by NASA Origins of the Solar System grant No. NMO7100830/102190, and NASA APRA grant No. 08-APRA08-0117. B.R.O. acknowledges continued support from Paco. Our team is also grateful to the Plymouth Hill Foundation, and an anonymous donor, as well as the efforts of Mike Werner, Paul Goldsmith, Jacob van Zyl, and Stephanie Hunt. E. L. R. acknowledges support from NASA through the American Astronomical Society's Small Research Grant Program. R.N. performed this work with funding through a grant from Helge Ax:son Johnson's foundation. L. P. performed this work in part under contract with the California Institute of Technology funded by NASA through the Sagan Fellowship Program. S. H. is supported by a National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under award No. AST-1203023. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. R. F. and D. W. H. were partially supported by the National Science Foundation under award No. IIS-1124794. B.R.O. thanks Didier Saumon and Mark Marley, as well as Bruce Macintosh, Gilles Chabrier and Isabelle Baraffe, as well as Jackie Faherty and Statia Cook, for comments and discussion of a draft prior to submission. We thank the Raymond and Beverly Sacker Foundation whose generous donation allowed the purchase of the original Project 1640 detector. We also thank Teledyne Imaging Sensors for their help and support throughout this project. We thank the dedication and assistance of Andy Boden, Shrinivas Kulkarni and Anna Marie Hetman at Caltech Optical Observatories. Finally, the entire team expresses sincere gratitude and appreciation for the hard work of the Palomar mountain crew, especially by Bruce Baker, Mike Doyle, Carolyn Heffner, John Henning, Greg van Idsinga, Steve Kunsman, Dan McKenna, Jean Mueller, Kajsa Peffer, Kevin Rykowski, and Pam Thompson. This project would be impossible without the flexibility, responsiveness and dedication of such an effective and motivated staff. A description of the contributions of each author can be found at http://www.amnh.org/project1640. NR 97 TC 66 Z9 67 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 24 DI 10.1088/0004-637X/768/1/24 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500024 ER PT J AU Pullen, AR Chang, TC Dore, O Lidz, A AF Pullen, Anthony R. Chang, Tzu-Ching Dore, Olivier Lidz, Adam TI CROSS-CORRELATIONS AS A COSMOLOGICAL CARBON MONOXIDE DETECTOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; diffuse radiation; intergalactic medium; large-scale structure of universe ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; MICROWAVE BACKGROUND-RADIATION; CO-LUMINOSITY FUNCTIONS; STAR-FORMATION HISTORY; RED GALAXY SAMPLE; DATA RELEASE; FORMING GALAXIES; ANGULAR MASKS; MOLECULAR GAS AB We present a new procedure to measure the large-scale carbon monoxide (CO) emissions across cosmic history. As a tracer of large-scale structure (LSS), the CO gas content as a function of redshift can be quantified by its three-dimensional fluctuation power spectra. Furthermore, cross-correlating CO emission with other LSS tracers offers a way to measure the emission as a function of scale and redshift. Here we introduce the model relevant for such a cross-correlation measurement between CO and other LSS tracers, and between different CO rotational lines. We propose a novel use of cosmic microwave background (CMB) data and attempt to extract redshifted CO emissions embedded in the Wilkinson Microwave Anisotropy Probe (WMAP) data set. We cross-correlate the all-sky WMAP7 data with LSS data sets, namely, the photometric quasar sample and the luminous red galaxy sample from the Sloan Digital Sky Survey Data Releases 6 and 7, respectively. We are unable to detect a cross-correlation signal with either CO(1-0) or CO(2-1) lines, mainly due to the instrumental noise in the WMAP data. However, we are able to rule out models more than three times greater than our more optimistic model. We discuss the cross-correlation signal from the thermal Sunyaev-Zeldovich effect and dust as potential contaminants, and quantify their impact for our CO measurements. We discuss forecasts for current CMB experiments and a hypothetical future CO-focused experiment, and propose to cross-correlate CO temperature data with the Hobby-Eberly Telescope Dark Energy Experiment Ly alpha-emitter sample, for which a signal-to-noise ratio of 58 is possible. C1 [Pullen, Anthony R.; Dore, Olivier] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Chang, Tzu-Ching] Acad Sinica, IAA, Taipei 10617, Taiwan. [Dore, Olivier] CALTECH, Pasadena, CA 91125 USA. [Lidz, Adam] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Pullen, AR (reprint author), CALTECH, NASA, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-237, Pasadena, CA 91109 USA. EM anthony.r.pullen@jpl.nasa.gov RI Pullen, Anthony/I-7007-2015 OI Pullen, Anthony/0000-0002-2091-8738 FU Keck Institute of Space Studies; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We thank D. Hanson, S. Furlanetto, and M. Seiffert for helpful comments and useful discussions. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. A. P. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. This work was supported by the Keck Institute of Space Studies and we thank colleagues at the "First Billion Years" for stimulating discussions, in particular J. Bowman and A. Readhead for organizing it.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 58 TC 14 Z9 14 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 MAY 1 PY 2013 VL 768 IS 1 AR 15 DI 10.1088/0004-637X/768/1/15 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500015 ER PT J AU Stefanon, M Marchesini, D Rudnick, GH Brammer, GB Whitaker, KE AF Stefanon, Mauro Marchesini, Danilo Rudnick, Gregory H. Brammer, Gabriel B. Whitaker, Katherine E. TI WHAT ARE THE PROGENITORS OF COMPACT, MASSIVE, QUIESCENT GALAXIES AT z=2.3? THE POPULATION OF MASSIVE GALAXIES AT z > 3 FROM NMBS AND CANDELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: structure ID SIMILAR-TO 2; STAR-FORMATION HISTORIES; HUBBLE-SPACE-TELESCOPE; INSIDE-OUT GROWTH; EXTRAGALACTIC LEGACY SURVEY; HIGH-REDSHIFT GALAXIES; STELLAR MASS; ELLIPTIC GALAXIES; SIZE EVOLUTION; COLOR-MAGNITUDE AB Using public data from the NEWFIRM Medium-Band Survey (NMBS) and the Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey (CANDELS), we investigate the population of massive galaxies at z > 3. The main aim of this work is to identify the potential progenitors of z similar to 2 compact, massive, quiescent galaxies (CMQGs), furthering our understanding of the onset and evolution of massive galaxies. Our work is enabled by high-resolution images from CANDELS data and accurate photometric redshifts, stellar masses, and star formation rates (SFRs) from 37-band NMBS photometry. The total number of massive galaxies at z > 3 is consistent with the number of massive, quiescent galaxies (MQGs) at z similar to 2, implying that the SFRs for all of these galaxies must be much lower by z similar to 2. We discover four CMQGs at z > 3, pushing back the time for which such galaxies have been observed. However, the volume density for these galaxies is significantly less than that of galaxies at z < 2 with similar masses, SFRs, and sizes, implying that additional CMQGs must be created in the intervening similar to 1 Gyr between z = 3 and z = 2. We find five star-forming galaxies at z similar to 3 that are compact (R-e < 1.4 kpc) and have stellar mass M-* > 10(10.6) M-circle dot; these galaxies are likely to become members of the massive, quiescent, compact galaxy population at z similar to 2. We evolve the stellar masses and SFRs of each individual z > 3 galaxy adopting five different star formation histories (SFHs) and studying the resulting population of massive galaxies at z = 2.3. We find that declining or truncated SFHs are necessary to match the observed number density of MQGs at z similar to 2, whereas a constant delayed-exponential SFH would result in a number density significantly smaller than observed. All of our assumed SFHs imply number densities of CMQGs at z similar to 2 that are consistent with the observed number density. Better agreement with the observed number density of CMQGs at z similar to 2 is obtained if merging is included in the analysis and better still if star formation quenching is assumed to shortly follow the merging event, as implied by recent models of the formation of MQGs. C1 [Stefanon, Mauro; Rudnick, Gregory H.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Brammer, Gabriel B.] European So Observ, Santiago 19, Chile. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Stefanon, M (reprint author), Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. EM stefanonm@missouri.edu RI Stefanon, Mauro/F-8708-2016 OI Stefanon, Mauro/0000-0001-7768-5309 FU National Science Foundation [EPS-0903806]; NSF; NASA; NASA [NAS5-26555]; Tufts University Mellon Research Fellowship FX The authors are thankful to the anonymous referee for comments and suggestions which helped to improve the paper. This material is based upon work supported by the National Science Foundation under Award No. EPS-0903806 and matching support from the State of Kansas through the Kansas Technology Enterprise Corporation. This study makes use of data from the NEWFIRM Medium-Band Survey, a multi-wavelength survey conducted with the NEWFIRM instrument at the KPNO, supported in part by NSF and NASA. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This research made use of the OSX Version of SCISOFT assembled by Dr. Nor Pirzkal and F. Pierfederici. D. M. acknowledges the support of the Tufts University Mellon Research Fellowship. NR 76 TC 20 Z9 20 U1 0 U2 2 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 MAY 1 PY 2013 VL 768 IS 1 AR 92 DI 10.1088/0004-637X/768/1/92 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500092 ER PT J AU Temim, T Slane, P Castro, D Plucinsky, PP Gelfand, J Dickel, JR AF Temim, Tea Slane, Patrick Castro, Daniel Plucinsky, Paul P. Gelfand, Joseph Dickel, John R. TI HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: ISM; ISM: individual objects (MSH 15-56, G326.1-1.8); ISM: supernova remnants; pulsars: general; X-rays: ISM ID LARGE-AREA TELESCOPE; PULSAR WIND NEBULA; CHANDRA OBSERVATIONS; EVOLUTION; CATALOG; G326.3-1.8; MODEL; RAY AB MSH 15-56 (G326.3-1.8) is a composite supernova remnant (SNR) that consists of an SNR shell and a displaced pulsar wind nebula (PWN) in the radio. We present XMM-Newton and Chandra X-ray observations of the remnant that reveal a compact source at the tip of the radio PWN and complex structures that provide evidence for mixing of the supernova (SN) ejecta with PWN material following a reverse shock interaction. The X-ray spectra are well fitted by a non-thermal power-law model whose photon index steepens with distance from the presumed pulsar, and a thermal component with an average temperature of 0.55 keV. The enhanced abundances of silicon and sulfur in some regions, and the similar temperature and ionization timescale, suggest that much of the X-ray emission can be attributed to SN ejecta that have either been heated by the reverse shock or swept up by the PWN. We find one region with a lower temperature of 0.3 keV that appears to be in ionization equilibrium. Assuming the Sedov model, we derive a number of SNR properties, including an age of 16,500 yr. Modeling of the gamma-ray emission detected by Fermi shows that the emission may originate from the reverse shock-crushed PWN. C1 [Temim, Tea] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Temim, Tea] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Slane, Patrick; Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Castro, Daniel] MIT Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Gelfand, Joseph] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Dickel, John R.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM tea.temim@nasa.gov RI Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Temim, Tea/0000-0001-7380-3144 FU NASA; NASA [NAS8-03060, NNX11AQ09G] FX T.T. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. P. S. and P. P. acknowledge partial support from NASA contract NAS8-03060, and P. S. acknowledges partial support from NASA grant NNX11AQ09G. NR 35 TC 4 Z9 4 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 MAY 1 PY 2013 VL 768 IS 1 AR 61 DI 10.1088/0004-637X/768/1/61 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500061 ER PT J AU Thacker, C Cooray, A Smidt, J De Bernardis, F Mitchell-Wynne, K Amblard, A Auld, R Baes, M Clements, DL Dariush, A De Zotti, G Dunne, L Eales, S Hopwood, R Hoyos, C Ibar, E Jarvis, M Maddox, S Michalowski, MJ Pascale, E Scott, D Serjeant, S Smith, MWL Valiante, E van der Werf, P AF Thacker, Cameron Cooray, Asantha Smidt, Joseph De Bernardis, Francesco Mitchell-Wynne, K. Amblard, A. Auld, R. Baes, M. Clements, D. L. Dariush, A. De Zotti, G. Dunne, L. Eales, S. Hopwood, R. Hoyos, C. Ibar, E. Jarvis, M. Maddox, S. Michalowski, M. J. Pascale, E. Scott, D. Serjeant, S. Smith, M. W. L. Valiante, E. van der Werf, P. TI H-ATLAS: THE COSMIC ABUNDANCE OF DUST FROM THE FAR-INFRARED BACKGROUND POWER SPECTRUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; infrared: galaxies; large-scale structure of universe; submillimeter: galaxies ID GALAXY NUMBER COUNTS; HERSCHEL-ATLAS; LUMINOSITY FUNCTION; SUBMILLIMETER LUMINOSITY; DARK-MATTER; INTERSTELLAR DUST; LOCAL UNIVERSE; LOW-REDSHIFT; MU-M; SPIRE AB We present a measurement of the angular power spectrum of the cosmic far-infrared background (CFIRB) anisotropies in one of the extragalactic fields of the Herschel Astrophysical Terahertz Large Area Survey at 250, 350, and 500 mu m bands. Consistent with recent measurements of the CFIRB power spectrum in Herschel-SPIRE maps, we confirm the existence of a clear one-halo term of galaxy clustering on arcminute angular scales with large-scale two-halo term of clustering at 30 arcmin to angular scales of a few degrees. The power spectrum at the largest angular scales, especially at 250 mu m, is contaminated by the Galactic cirrus. The angular power spectrum is modeled using a conditional luminosity function approach to describe the spatial distribution of unresolved galaxies that make up the bulk of the CFIRB. Integrating over the dusty galaxy population responsible for the background anisotropies, we find that the cosmic abundance of dust, relative to the critical density, to be between Omega(dust) = 10-6 and 8 x 10(-6) in the redshift range z similar to 0-3. This dust abundance is consistent with estimates of the dust content in the universe using quasar reddening and magnification measurements in the Sloan Digital Sky Survey. C1 [Thacker, Cameron; Cooray, Asantha; Smidt, Joseph; De Bernardis, Francesco; Mitchell-Wynne, K.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Auld, R.; Eales, S.; Pascale, E.; Smith, M. W. L.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Baes, M.; Michalowski, M. J.] Univ Ghent, B-9000 Ghent, Belgium. [Clements, D. L.; Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [De Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Hoyos, C.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ibar, E.] Catholic Univ Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Jarvis, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Michalowski, M. J.] Univ Edinburgh, Royal Observ, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Serjeant, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Thacker, C (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RI Baes, Maarten/I-6985-2013; amblard, alexandre/L-7694-2014; OI Baes, Maarten/0000-0002-3930-2757; amblard, alexandre/0000-0002-2212-5395; De Zotti, Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X; Scott, Douglas/0000-0002-6878-9840; De Hoyos Fernandez De Cordova, Carlos/0000-0003-3120-6856 FU NSF CAREER [AST-0645427]; NASA at UCI [NNX10AD42G] FX We thank Brice Menard and Marco Viero for useful discussions. The Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS Web site is http://www.h-atlas.org/. This work was supported by NSF CAREER AST-0645427 and NASA NNX10AD42G at UCI to A. C., and support for US Participants in Herschel programs from NASA Herschel Science Center/JPL. NR 72 TC 13 Z9 13 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 58 DI 10.1088/0004-637X/768/1/58 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500058 ER PT J AU Weiss, LM Marcy, GW Rowe, JF Howard, AW Isaacson, H Fortney, JJ Miller, N Demory, BO Fischer, DA Adams, ER Dupree, AK Howell, SB Kolbl, R Johnson, JA Horch, EP Everett, ME Fabrycky, DC Seager, S AF Weiss, Lauren M. Marcy, Geoffrey W. Rowe, Jason F. Howard, Andrew W. Isaacson, Howard Fortney, Jonathan J. Miller, Neil Demory, Brice-Olivier Fischer, Debra A. Adams, Elisabeth R. Dupree, Andrea K. Howell, Steve B. Kolbl, Rea Johnson, John Asher Horch, Elliott P. Everett, Mark E. Fabrycky, Daniel C. Seager, Sara TI THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: composition; stars: individual (KOI, 94, KIC 6462863, 2MASS J19491993+4153280); techniques: photometric; techniques: spectroscopic ID COROT SPACE MISSION; TRANSITING HOT JUPITER; LOW-DENSITY PLANET; SOLAR-TYPE STAR; SUN-LIKE STAR; HOBBY-EBERLY TELESCOPE; FOLLOW-UP PROGRAM; GAS-GIANT PLANET; METAL-POOR STAR; B-LIKE PLANETS AB We measure the mass of a modestly irradiated giant planet, KOI-94d. We wish to determine whether this planet, which is in a 22 day orbit and receives 2700 times as much incident flux as Jupiter, is as dense as Jupiter or rarefied like inflated hot Jupiters. KOI-94 also hosts at least three smaller transiting planets, all of which were detected by the Kepler mission. With 26 radial velocities of KOI-94 from the W.M. Keck Observatory and a simultaneous fit to the Kepler light curve, we measure the mass of the giant planet and determine that it is not inflated. Support for the planetary interpretation of the other three candidates comes from gravitational interactions through transit timing variations, the statistical robustness of multi-planet systems against false positives, and several lines of evidence that no other star resides within the photometric aperture. We report the properties of KOI-94b (M-P = 10.5 +/- 4.6 M-circle plus, R-P = 1.71 +/- 0.16 R-circle plus, P = 3.74 days), KOI-94c (M-P = 15.6(15.6)(+5.7) M-circle plus, R-P = 4.32 +/- 0.41 R-circle plus, P = 10.4 days), KOI-94d (M-P = 106 +/- 11 M-circle plus, R-P = 11.27 +/- 1.06 R-circle plus, P = 22.3 days), and KOI-94e (M-P = 35(-28)(+18) M-circle plus, R-P = 6.56 +/- 0.62 R-circle plus, P = 54.3 days). The radial velocity analyses of KOI-94b and KOI-94e offer marginal (>2 sigma) mass detections, whereas the observations of KOI-94c offer only an upper limit to its mass. Using the KOI-94 system and other planets with published values for both mass and radius (138 exoplanets total, including 35 with M-P < 150 M-circle plus), we establish two fundamental planes for exoplanets that relate their mass, incident flux, and radius from a few Earth masses up to 13 Jupiter masses: (R-P/R-circle plus) = 1.78(M-P/M-circle plus) 0.53(F/erg s(-1) cm(-2))(-0.03) for M-P < 150 M-circle plus, and R-P/R-circle plus = 2.45(M-P/M-circle plus)(-0.039)(F/erg s(-1) cm(-2))(0.094) for M-P > 150 M-circle dot. These equations can be used to predict the radius or mass of a planet. C1 [Weiss, Lauren M.; Marcy, Geoffrey W.; Isaacson, Howard; Kolbl, Rea] Univ Calif Berkeley, Dept Astron, Hearst Field Annex B 20, Berkeley, CA 94720 USA. [Rowe, Jason F.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Fortney, Jonathan J.; Miller, Neil] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Demory, Brice-Olivier; Seager, Sara] MIT, Cambridge, MA 02139 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06510 USA. [Adams, Elisabeth R.; Dupree, Andrea K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johnson, John Asher] CALTECH, Pasadena, CA 91106 USA. [Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Weiss, LM (reprint author), Univ Calif Berkeley, Dept Astron, Hearst Field Annex B 20, 601 Campbell Hall, Berkeley, CA 94720 USA. EM lweiss@berkeley.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Weiss, Lauren/0000-0002-3725-3058; Demory, Brice-Olivier/0000-0002-9355-5165; Fabrycky, Daniel/0000-0003-3750-0183 FU NSF [DGE 1106400] FX L.M.W. is financially supported by the National Science Foundation Graduate Research Fellowship Program, Grant DGE 1106400. NR 177 TC 90 Z9 91 U1 2 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 MAY 1 PY 2013 VL 768 IS 1 AR 14 DI 10.1088/0004-637X/768/1/14 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500014 ER PT J AU Rio, C Grandpeix, JY Hourdin, F Guichard, F Couvreux, F Lafore, JP Fridlind, A Mrowiec, A Roehrig, R Rochetin, N Lefebvre, MP Idelkadi, A AF Rio, Catherine Grandpeix, Jean-Yves Hourdin, Frederic Guichard, Francoise Couvreux, Fleur Lafore, Jean-Philippe Fridlind, Ann Mrowiec, Agnieszka Roehrig, Romain Rochetin, Nicolas Lefebvre, Marie-Pierre Idelkadi, Abderrahmane TI Control of deep convection by sub-cloud lifting processes: the ALP closure in the LMDZ5B general circulation model SO CLIMATE DYNAMICS LA English DT Article DE Deep convection parameterization; Triggering and closure; Oceanic versus continental convection; Diurnal cycle of precipitation; High resolution simulations to evaluate parameterizations assumptions ID SHALLOW CUMULUS CONVECTION; VERTICAL VELOCITY EVENTS; LARGE-SCALE MODELS; MASS-FLUX; BOUNDARY-LAYER; PART I; WAKE PARAMETERIZATION; OCEANIC CONVECTION; SCHEME; SIMULATIONS AB Recently, a new conceptual framework for deep convection scheme triggering and closure has been developed and implemented in the LMDZ5B general circulation model, based on the idea that deep convection is controlled by sub-cloud lifting processes. Such processes include boundary-layer thermals and evaporatively-driven cold pools (wakes), which provide an available lifting energy that is compared to the convective inhibition to trigger deep convection, and an available lifting power (ALP) at cloud base, which is used to compute the convective mass flux assuming the updraft vertical velocity at the level of free convection. While the ALP closure was shown to delay the local hour of maximum precipitation over land in better agreement with observations, it results in an underestimation of the convection intensity over the tropical ocean both in the 1D and 3D configurations of the model. The specification of the updraft vertical velocity at the level of free convection appears to be a key aspect of the closure formulation, as it is weaker over tropical ocean than over land and weaker in moist mid-latitudes than semi-arid regions. We propose a formulation making this velocity increase with the level of free convection, so that the ALP closure is adapted to various environments. Cloud-resolving model simulations of observed oceanic and continental case studies are used to evaluate the representation of lifting processes and test the assumptions at the basis of the ALP closure formulation. Results favor closures based on the lifting power of sub-grid sub-cloud processes rather than those involving quasi-equilibrium with the large-scale environment. The new version of the model including boundary-layer thermals and cold pools coupled together with the deep convection scheme via the ALP closure significantly improves the representation of various observed case studies in 1D mode. It also substantially modifies precipitation patterns in the full 3D version of the model, including seasonal means, diurnal cycle and intraseasonal variability. C1 [Rio, Catherine] UPMC, Lab Meteorol Dynam, CNRS, IPSL, F-75005 Paris, France. [Grandpeix, Jean-Yves; Hourdin, Frederic; Roehrig, Romain; Rochetin, Nicolas; Idelkadi, Abderrahmane] LMD, Paris, France. [Guichard, Francoise; Couvreux, Fleur; Lafore, Jean-Philippe] GAME, CNRM, Toulouse, France. [Fridlind, Ann; Mrowiec, Agnieszka] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Lefebvre, Marie-Pierre] CNRM, LMD, Paris, France. RP Rio, C (reprint author), UPMC, Lab Meteorol Dynam, CNRS, IPSL, Tr 45-55,3E & B99 Jussieu, F-75005 Paris, France. EM catherine.rio@lmd.jussieu.fr NR 55 TC 23 Z9 23 U1 0 U2 15 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD MAY PY 2013 VL 40 IS 9-10 SI SI BP 2271 EP 2292 DI 10.1007/s00382-012-1506-x PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 135HH UT WOS:000318278700008 ER PT J AU Soibel, A Rafol, SB Khoshakhlagh, A Nguyen, J Hoeglund, L Keo, SA Mumolo, JM Liu, J Liao, A Ting, DZY Gunapala, SD AF Soibel, A. Rafol, S. B. Khoshakhlagh, Arezou Nguyen, Jean Hoeglund, Linda Keo, Sam A. Mumolo, Jason M. Liu, John Liao, Anna Ting, David Z. -Y. Gunapala, Sarath D. TI Long Wavelength Infrared Superlattice Detectors and FPAs Based on CBIRD Design SO IEEE PHOTONICS TECHNOLOGY LETTERS LA English DT Article DE Focal plane array (FPA); infrared; long wavelength infrared; superlattice detectors ID SUPER-LATTICE; PERFORMANCE AB In this letter, we demonstrate the next generation of N+-p complementary barrier infrared detectors (nCBIRD) with 9.9 mu m cutoff wavelength that have near zero bias operation and exhibit dark current density of 6 x 10(-6) A/cm(2) at 77 K. These nCBIRDs have been recently utilized in the 320 x 256 focal plane array that exhibited a noise equivalent differential temperature of 18.6 mK at an operating temperature of 77 K, with a 300 K background and f/2 cold-stop. We compare single pixel photodiode characteristics with the performance of FPAs that were fabricated together on the same wafer. This letter identifies the physical processes affecting the performance of long wave infrared photodetectors based on CBIRD design. C1 [Soibel, A.; Rafol, S. B.; Khoshakhlagh, Arezou; Nguyen, Jean; Hoeglund, Linda; Keo, Sam A.; Mumolo, Jason M.; Liu, John; Liao, Anna; Ting, David Z. -Y.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Ctr Infrared Sensors, Pasadena, CA 91109 USA. RP Soibel, A (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Sensors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM asoibel@jpl.nasa.gov; sir.b.rafol@jpl.nasa.gov; Arezou.Khoshakhlagh@jpl.nasa.gov; jean.nguyen@jpl.nasa.gov; linda.hoglund@jpl.nasa.gov; Sam.A.Keo@jpl.nasa.gov; jason.m.mumolo@jpl.nasa.gov; John.k.liu@jpl.nasa.gov; ALLiao@lbl.gov; david.z.ting@jpl.nasa.gov; sarath.d.gunapala@jpl.nasa.gov RI Soibel, Alexander/A-1313-2007 FU Missile Defense Agency; National Aeronautics and Space Administration FX This work was supported by the Missile Defense Agency. The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 15 TC 7 Z9 7 U1 2 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1041-1135 J9 IEEE PHOTONIC TECH L JI IEEE Photonics Technol. Lett. PD MAY 1 PY 2013 VL 25 IS 9 BP 875 EP 878 DI 10.1109/LPT.2013.2254111 PG 4 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 133VJ UT WOS:000318168600010 ER PT J AU Kato, S Loeb, NG Rose, FG Doelling, DR Rutan, DA Caldwell, TE Yu, LS Weller, RA AF Kato, Seiji Loeb, Norman G. Rose, Fred G. Doelling, David R. Rutan, David A. Caldwell, Thomas E. Yu, Lisan Weller, Robert A. TI Surface Irradiances Consistent with CERES-Derived Top-of-Atmosphere Shortwave and Longwave Irradiances SO JOURNAL OF CLIMATE LA English DT Article ID ENERGY-SYSTEM CERES; SEA-SURFACE; RADIATION BUDGET; OBSERVING SYSTEM; CLOUD; EMISSIVITY; SATELLITE; CLIMATE; CALIPSO; FLUX AB The estimate of surface irradiance on a global scale is possible through radiative transfer calculations using satellite-retrieved surface, cloud, and aerosol properties as input. Computed top-of-atmosphere (TOA) irradiances, however, do not necessarily agree with observation-based values, for example, from the Clouds and the Earth's Radiant Energy System (CERES). This paper presents a method to determine surface irradiances using observational constraints of TOA irradiance from CERES. A Lagrange multiplier procedure is used to objectively adjust inputs based on their uncertainties such that the computed TOA irradiance is consistent with CERES-derived irradiance to within the uncertainty. These input adjustments are then used to determine surface irradiance adjustments. Observations by the Atmospheric Infrared Sounder (AIRS), Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO), CloudSat, and Moderate Resolution Imaging Spectroradiometer (MODIS) that are a part of the NASA A-Train constellation provide the uncertainty estimates. A comparison with surface observations from a number of sites shows that the bias [root-mean-square (RMS) difference] between computed and observed monthly mean irradiances calculated with 10 years of data is 4.7 (13.3) W m(-2) for downward shortwave and -2.5 (7.1) W m(-2) for downward longwave irradiances over ocean and -1.7 (7.8) W m(-2) for downward shortwave and -1.0 (7.6) W m(-2) for downward longwave irradiances over land. The bias and RMS error for the downward longwave and shortwave irradiances over ocean are decreased from those without constraint. Similarly, the bias and RMS error for downward longwave over land improves, although the constraint does not improve downward shortwave over land. This study demonstrates how synergetic use of multiple instruments (CERES, MODIS, CALIPSO, CloudSat, AIRS, and geostationary satellites) improves the accuracy of surface irradiance computations. C1 [Kato, Seiji; Loeb, Norman G.; Doelling, David R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Rose, Fred G.] Sci Syst & Applicat Inc, Hampton, VA USA. [Rutan, David A.; Caldwell, Thomas E.] Sci Syst & Applicat Inc, Lanham, MD USA. [Yu, Lisan; Weller, Robert A.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. RP Kato, S (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM seiji.kato@nasa.gov OI Rose, Fred G/0000-0003-0769-0772 FU NASA CERES project; NASA Energy Water Cycle Study (NEWS) project FX We thank Dr. Bjorn Stevens for useful discussions and Drs. Paul Stackhouse and Shashi Gupta for providing Flashflux data. The work was supported by the NASA CERES and, in part, Energy Water Cycle Study (NEWS) projects. NR 52 TC 90 Z9 91 U1 3 U2 51 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAY PY 2013 VL 26 IS 9 BP 2719 EP 2740 DI 10.1175/JCLI-D-12-00436.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 133SH UT WOS:000318159500002 ER PT J AU Wahid, N Bounoua, L AF Wahid, Nadya Bounoua, Lahouari TI The relationship between seed weight, germination and biochemical reserves of maritime pine (Pinus pinaster Ait.) in Morocco SO NEW FORESTS LA English DT Article DE Maritime pine; Seed weight; Germination capacity; Biochemical reserves ID NATURAL-POPULATIONS; GENETIC-CONTROL; DOUGLAS-FIR; SIZE; PROTEIN; GROWTH; EMBRYO; SUGARS AB Seed germination and biochemical reserves of maritime pine (Pinus pinaster Ait.) were studied with the aim of providing germination information for reforestation and conservation programs. Ten natural populations were used to assess variation in seed weight, germination characteristics and biochemical reserves and to examine the relationship between these characteristics. The analysis of variance showed highly significant population effects for seed weight, germination characteristics and protein content in both seeds and the female gametophyte. The mobilization of protein content in female gametophyte during seed germination differed more among populations than sugar content, suggesting that protein content was more sensitive to environment effects than sugar content. A strong positive correlation between germination capacity and the protein content in both seeds and female gametophyte indicated that the best populations in term of germination capacity may also be the richest in protein content. Seeds that were heavier and had a lower speed of protein content mobilization in the female gametophyte appeared to be better adapted to drought conditions. The results also suggested that as much as possible of the potentially valuable genetic variation among populations of this species should be preserved for reforestation and conservation purposes. C1 [Wahid, Nadya] Univ Sidi Mohamed Ben Abdellah, Inst Natl Plantes Med & Aromat, Taounate 34000, Morocco. [Bounoua, Lahouari] NASA, Goddard Space Flight Ctr, Biospher Sci Lab Code 618, Greenbelt, MD 20771 USA. RP Wahid, N (reprint author), Univ Sidi Mohamed Ben Abdellah, Inst Natl Plantes Med & Aromat, BP 159, Taounate 34000, Morocco. EM wahid2na@yahoo.fr NR 42 TC 5 Z9 6 U1 5 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-4286 J9 NEW FOREST JI New For. PD MAY PY 2013 VL 44 IS 3 BP 385 EP 397 DI 10.1007/s11056-012-9348-2 PG 13 WC Forestry SC Forestry GA 131OR UT WOS:000318003500006 ER PT J AU Gopalswamy, N Nieves-Chinchilla, T Hidalgo, M Zhang, J Riley, P van Driel-Gesztelyi, L Mandrini, CH AF Gopalswamy, N. Nieves-Chinchilla, T. Hidalgo, M. Zhang, J. Riley, P. van Driel-Gesztelyi, L. Mandrini, C. H. TI Flux-Rope Structure of Coronal Mass Ejections Preface SO SOLAR PHYSICS LA English DT Editorial Material C1 [Gopalswamy, N.; Nieves-Chinchilla, T.] NASA Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD USA. [Nieves-Chinchilla, T.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Hidalgo, M.] SRG UAH, Madrid, Spain. [Zhang, J.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Riley, P.] Predict Sci Inc, San Diego, CA USA. [van Driel-Gesztelyi, L.] Observ Paris, LESIA CNRS UMR 8109, F-9295 Meudon, France. [van Driel-Gesztelyi, L.] Univ Coll London, Mullard Space Sci Lab, Holmbury, England. [van Driel-Gesztelyi, L.] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary. [Mandrini, C. H.] CONICET UBA, Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. RP Gopalswamy, N (reprint author), NASA Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD USA. EM nat.gopalswamy@nasa.gov RI Nieves-Chinchilla, Teresa/F-3482-2016 OI Nieves-Chinchilla, Teresa/0000-0003-0565-4890 NR 2 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 1 EP 4 DI 10.1007/s11207-013-0280-1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300001 ER PT J AU Yashiro, S Gopalswamy, N Makela, P Akiyama, S AF Yashiro, S. Gopalswamy, N. Maekelae, P. Akiyama, S. TI Post-Eruption Arcades and Interplanetary Coronal Mass Ejections SO SOLAR PHYSICS LA English DT Article DE Flares; Coronal mass ejections; Posteruption arcades; Flux rope; Magnetic cloud ID X-RAY; MAGNETIC RECONNECTION; SOLAR-FLARES; RADIO; MODEL; LOOP; ASSOCIATION; PROMINENCES; PARAMETERS AB We compare the temporal and spatial properties of posteruption arcades (PEAs) associated with coronal mass ejections (CMEs) at the Sun that end up as magnetic cloud (MC) and non-MC events in the solar wind. We investigate the length, width, area, tilt angle, and formation time of the PEAs associated with 22 MC and 29 non-MC events and we find no difference between the two populations. According to current ideas on the relation between flares and CMEs, the PEA is formed together with the CME flux-rope structure by magnetic reconnection. Our results indicate that at the Sun flux ropes form during CMEs in association with both MC and non-MC events; however, for non-MC events the flux-rope structure is not observed in the interplanetary space because of the geometry of the observation, i.e. the location of the spacecraft when the structure passes through it. C1 [Yashiro, S.; Maekelae, P.; Akiyama, S.] Catholic Univ Amer, Washington, DC 20064 USA. [Yashiro, S.; Gopalswamy, N.; Maekelae, P.; Akiyama, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yashiro, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM seiji.yashiro@nasa.gov; nat.gopalswamy@nasa.gov; pertti.makela@nasa.gov; sachiko.akiyama@nasa.gov FU NASA [NNX10AL50A, NNG11PL10A] FX We would like to thank the local organizers of the LWS CDAW meetings in San Diego, USA, and Alcala de Henares, Spain. This research was supported by NASA grants NNX10AL50A and NNG11PL10A. SOHO is an international cooperation project between ESA and NASA. NR 34 TC 9 Z9 9 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 5 EP 15 DI 10.1007/s11207-013-0248-1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300002 ER PT J AU Gopalswamy, N Makela, P Akiyama, S Xie, H Yashiro, S Reinard, AA AF Gopalswamy, N. Maekelae, P. Akiyama, S. Xie, H. Yashiro, S. Reinard, A. A. TI The Solar Connection of Enhanced Heavy Ion Charge States in the Interplanetary Medium: Implications for the Flux-Rope Structure of CMEs SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections; Flares; Flux rope; Magnetic cloud, charge state ID CORONAL MASS EJECTIONS; II RADIO-BURSTS; MAGNETIC RECONNECTION; FLARE; PLASMA; CLOUD; WIND AB We investigated a set of 54 interplanetary coronal mass ejection (ICME) events whose solar sources are very close to the disk center (within +/- 15(a similar to) from the central meridian). The ICMEs consisted of 23 magnetic-cloud (MC) events and 31 non-MC events. Our analyses suggest that the MC and non-MC ICMEs have more or less the same eruption characteristics at the Sun in terms of soft X-ray flares and CMEs. Both types have significant enhancements in ion charge states, although the non-MC structures have slightly lower levels of enhancement. The overall duration of charge-state enhancement is also considerably smaller than that in MCs as derived from solar wind plasma and magnetic signatures. We find very good correlation between the Fe and O charge-state measurements and the flare properties such as soft X-ray flare intensity and flare temperature for both MCs and non-MCs. These observations suggest that both MC and non-MC ICMEs are likely to have a flux-rope structure and the unfavorable observational geometry may be responsible for the appearance of non-MC structures at 1 AU. We do not find any evidence for an active region expansion resulting in ICMEs lacking a flux-rope structure because the mechanism of producing high charge states and the flux-rope structure at the Sun is the same for MC and non-MC events. C1 [Gopalswamy, N.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Maekelae, P.; Akiyama, S.; Xie, H.; Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA. [Reinard, A. A.] NOAA Space Weather Predict Ctr, Boulder, CO USA. RP Gopalswamy, N (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD USA. EM nat.gopalswamy@nasa.gov RI Reinard, Alysha/H-7808-2013 OI Reinard, Alysha/0000-0003-0304-2989 NR 47 TC 12 Z9 12 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 17 EP 46 DI 10.1007/s11207-012-0215-2 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300003 ER PT J AU Xie, H Gopalswamy, N St Cyr, OC AF Xie, H. Gopalswamy, N. St Cyr, O. C. TI Near-Sun Flux-Rope Structure of CMEs SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections; Initiation and propagation ID CORONAL MASS EJECTIONS; LASCO AB We have used the Krall flux-rope model (Krall and St. Cyr, Astrophys. J. 2006, 657, 1740) (KFR) to fit 23 magnetic cloud (MC)-CMEs and 30 non-cloud ejecta (EJ)-CMEs in the Living With a Star (LWS) Coordinated Data Analysis Workshop (CDAW) 2011 list. The KFR-fit results shows that the CMEs associated with MCs (EJs) have been deflected closer to (away from) the solar disk center (DC), likely by both the intrinsic magnetic structures inside an active region (AR) and ambient magnetic structures (e.g. nearby ARs, coronal holes, and streamers, etc.). The mean absolute propagation latitudes and longitudes of the EJ-CMEs (18(a similar to), 11(a similar to)) were larger than those of the MC-CMEs (11(a similar to), 6(a similar to)) by 7(a similar to) and 5(a similar to), respectively. Furthermore, the KFR-fit widths showed that the MC-CMEs are wider than the EJ-CMEs. The mean fitting face-on width and edge-on width of the MC-CMEs (EJ-CMEs) were 87 (85)(a similar to) and 70 (63)(a similar to), respectively. The deflection away from DC and narrower angular widths of the EJ-CMEs have caused the observing spacecraft to pass over only their flanks and miss the central flux-rope structures. The results of this work support the idea that all CMEs have a flux-rope structure. C1 [Xie, H.] NASA, Goddard Flight Ctr, Solar Phys Lab, IACS CUA, Greenbelt, MD 20771 USA. [Gopalswamy, N.; St Cyr, O. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Xie, H (reprint author), NASA, Goddard Flight Ctr, Solar Phys Lab, IACS CUA, Greenbelt, MD 20771 USA. EM hong.xie@nasa.gov; nat.gopalswamy@nasa.gov; chris.stcyr@nasa.gov FU NASA [LWSTRT08-0029] FX This work uses data from the NASA/LWS Coordinated Data Analysis Workshops on CME/flux-ropes in 2010 and 2011. We acknowledge the workshop support provided by NASA/LWS, Predictive Sciences, Inc. (San Diego, CA), University of Alcala (Alcala de Henares, Spain), and Ministerio de Ciencia e Innovacion (Reference number AYA2010-12439-E), Spain. The authors acknowledge support of NASA grant LWSTRT08-0029. NR 20 TC 15 Z9 16 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 47 EP 58 DI 10.1007/s11207-012-0209-0 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300004 ER PT J AU Makela, P Gopalswamy, N Xie, H Mohamed, AA Akiyama, S Yashiro, S AF Maekelae, P. Gopalswamy, N. Xie, H. Mohamed, A. A. Akiyama, S. Yashiro, S. TI Coronal Hole Influence on the Observed Structure of Interplanetary CMEs SO SOLAR PHYSICS LA English DT Article DE Sun; Coronal holes; Coronal mass ejections; Magnetic clouds; Ejecta ID MASS EJECTIONS; SOLAR; DEFLECTION; SIGNATURES; SHOCKS AB We report on the coronal hole (CH) influence on the 54 magnetic cloud (MC) and non-MC associated coronal mass ejections (CMEs) selected for studies during the Coordinated Data Analysis Workshops (CDAWs) focusing on the question if all CMEs are flux ropes. All selected CMEs originated from source regions located between longitudes 15E -15W. Xie, Gopalswamy, and St. Cyr (2013, Solar Phys., doi: 10.1007/s11207-012-0209-0) found that these MC and non-MC associated CMEs are on average deflected towards and away from the Sun-Earth line, respectively. We used a CH influence parameter (CHIP) that depends on the CH area, average magnetic field strength, and distance from the CME source region to describe the influence of all on-disk CHs on the erupting CME. We found that for CHIP values larger than 2.6 G the MC and non-MC events separate into two distinct groups where MCs (non-MCs) are deflected towards (away) from the disk center. Division into two groups was also observed when the distance to the nearest CH was less than 3.2x10(5) km. At CHIP values less than 2.6 G or at distances of the nearest CH larger than 3.2x10(5) km the deflection distributions of the MC and non-MCs started to overlap, indicating diminishing CH influence. These results give support to the idea that all CMEs are flux ropes, but those observed to be non-MCs at 1 AU could be deflected away from the Sun-Earth line by nearby CHs, making their flux rope structure unobservable at 1 AU. C1 [Maekelae, P.; Xie, H.; Mohamed, A. A.; Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA. [Maekelae, P.; Gopalswamy, N.; Xie, H.; Mohamed, A. A.; Akiyama, S.; Yashiro, S.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Makela, P (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM pertti.makela@nasa.gov; nat.gopalswamy@nasa.gov; hong.xie@nasa.gov; amaal.shahin@nasa.gov; sachiko.akiyama@nasa.gov; seiji.yashiro@nasa.gov FU NASA [NNX10AL50A, NNG11PL10A] FX We would like to thank the local organizers of the LWS CDAW meetings in San Diego, USA, and Alcala de Henares, Spain. This research was supported by NASA grants NNX10AL50A and NNG11PL10A. SOHO is an international cooperation project between ESA and NASA. NR 30 TC 15 Z9 15 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 59 EP 75 DI 10.1007/s11207-012-0211-6 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300005 ER PT J AU Kim, RS Gopalswamy, N Cho, KS Moon, YJ Yashiro, S AF Kim, R. -S. Gopalswamy, N. Cho, K. -S. Moon, Y. -J. Yashiro, S. TI Propagation Characteristics of CMEs Associated with Magnetic Clouds and Ejecta SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections, ejecta; Interplanetary coronal mass ejections, magnetic clouds ID CORONAL MASS EJECTIONS; SOLAR-WIND; SHOCK AB We have investigated the characteristics of magnetic cloud (MC) and ejecta (EJ) associated coronal mass ejections (CMEs) based on the assumption that all CMEs have a flux rope structure. For this, we used 54 CMEs and their interplanetary counterparts (interplanetary CMEs: ICMEs) that constitute the list of events used by the NASA/LWS Coordinated Data Analysis Workshop (CDAW) on CME flux ropes. We considered the location, angular width, and speed as well as the direction parameter, D. The direction parameter quantifies the degree of asymmetry of the CME shape in coronagraph images, and shows how closely the CME propagation is directed to Earth. For the 54 CDAW events, we found the following properties of the CMEs: i) the average value of D for the 23 MCs (0.62) is larger than that for the 31 EJs (0.49), which indicates that the MC-associated CMEs propagate more directly toward the Earth than the EJ-associated CMEs; ii) comparison between the direction parameter and the source location shows that the majority of the MC-associated CMEs are ejected along the radial direction, while many of the EJ-associated CMEs are ejected non-radially; iii) the mean speed of MC-associated CMEs (946 km s(-1)) is faster than that of EJ-associated CMEs (771 km s(-1)). For seven very fast CMEs (a parts per thousand yenaEuro parts per thousand 1500 km s(-1)), all CMEs with large D (a parts per thousand yenaEuro parts per thousand 0.4) are associated with MCs and the CMEs with small D are associated with EJs. From the statistical analysis of CME parameters, we found the superiority of the direction parameter. Based on these results, we suggest that the CME trajectory essentially determines the observed ICME structure. C1 [Kim, R. -S.; Cho, K. -S.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Gopalswamy, N.; Yashiro, S.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea. [Yashiro, S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Kim, RS (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM rskim@kasi.re.kr RI Moon, Yong-Jae/E-1711-2013 FU Construction of Korean Space Weather Center of KASI; KASI Basic Research Fund; KRCF; WCU program through the National Research Foundation of Korea [R31-10016]; Basic Research Promotion Fund through the National Research Foundation of Korea [20090071744, 20100014501]; Ministry of Education, Science and Technology FX This work benefited from the NASA/LWS Coordinated Data Analysis Workshops on CME flux ropes in 2010 and 2011. We acknowledge the workshop support provided by NASA/LWS, Predictive Sciences, Inc. (San Diego, CA), University of Alcala (Alcala de Henares, Spain), and Ministerio de Ciencia e Innovacion (Reference number AYA2010-12439-E), Spain. This work was partially supported by the Construction of Korean Space Weather Center as the project of KASI, the KASI Basic Research Fund, and Research Fellowship for Young Scientists of KRCF. Y.-J.M. has been supported by the WCU program (No. R31-10016) and Basic Research Promotion Fund (20090071744 and 20100014501) through the National Research Foundation of Korea funded by the Ministry of Education, Science and Technology. NR 19 TC 8 Z9 8 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 77 EP 88 DI 10.1007/s11207-013-0230-y PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300006 ER PT J AU Zhang, J Hess, P Poomvises, W AF Zhang, J. Hess, P. Poomvises, W. TI A Comparative Study of Coronal Mass Ejections with and Without Magnetic Cloud Structure near the Earth: Are All Interplanetary CMEs Flux Ropes? SO SOLAR PHYSICS LA English DT Article ID SOLAR-FLARES; GEOMAGNETIC STORMS; CONE MODEL; SHOCK; EVOLUTION; ONSET; WIND; TEMPERATURE; PROPAGATION; SIGNATURES AB An outstanding question concerning interplanetary coronal mass ejections (ICMEs) is whether all ICMEs have a magnetic flux rope structure. We test this question by studying two different ICMEs, one having a magnetic cloud (MC) showing smooth rotation of magnetic field lines and the other not. The two ICMEs are chosen in such a way that their progenitor CMEs are very similar in remote sensing observations. Both CMEs originated from close to the central meridian directly facing the Earth. Both CMEs were associated with a long-lasting post-eruption loop arcade and appeared as an elliptical halo in coronagraph images, indicating a flux rope origin. We conclude that the difference in the in-situ observation is caused by the geometric selection effect, contributed by the deflection of flux ropes in the inner corona and interplanetary space. The first event had its nose pass through the observing spacecraft; thus, the intrinsic flux rope structure of the CME appeared as a magnetic cloud. On the other hand, the second event had the flank of the flux rope intercept the spacecraft, and it thus did not appear as a magnetic cloud. We further argue that a conspicuous long period of weak magnetic field, low plasma temperature, and density in the second event should correspond to the extended leg portion of the embedded magnetic flux rope, thus validating the scenario of the flank-passing. These observations support the idea that all CMEs arriving at the Earth include flux rope drivers. C1 [Zhang, J.; Hess, P.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Poomvises, W.] Catholic Univ Amer, Washington, DC 20064 USA. [Poomvises, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhang, J (reprint author), George Mason Univ, Sch Phys Astron & Computat Sci, 4400 Univ Dr,MSN 6A2, Fairfax, VA 22030 USA. EM jzhang7@gmu.edu FU NSF [ATM-0748003, AGS-1156120] FX We acknowledge the support from NSF ATM-0748003 and NSF AGS-1156120. The ACE plasma, magnetic field, and composition/charge state data were provided by the ACE Science Center. SOHO is a project of international cooperation between ESA and NASA. The LASCO instrument was constructed by a consortium of the Naval Research Laboratory, University of Birmingham (England), the Max-Planck-Institute fur Aeronomie (Germany) and the Laboratoire d'Astronomie Spatiale (France). NR 54 TC 6 Z9 6 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 89 EP 104 DI 10.1007/s11207-013-0242-7 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300007 ER PT J AU Cho, KS Park, SH Marubashi, K Gopalswamy, N Akiyama, S Yashiro, S Kim, RS Lim, EK AF Cho, K. -S. Park, S. -H. Marubashi, K. Gopalswamy, N. Akiyama, S. Yashiro, S. Kim, R. -S. Lim, E. -K. TI Comparison of Helicity Signs in Interplanetary CMEs and Their Solar Source Regions SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections; Magnetic cloud; Photospheric helicity; Solar surface magnetic field; Interplanetary magnetic field ID CORONAL MASS EJECTIONS; MAGNETIC HELICITY; FLUX ROPES; GEOMAGNETIC STORMS; ACTIVE REGIONS; CLOUDS; FILAMENTS; FIELDS; BUDGET; LASCO AB If all coronal mass ejections (CMEs) have flux ropes, then the CMEs should keep their helicity signs from the Sun to the Earth according to the helicity conservation principle. This study presents an attempt to answer the question from the Coordinated Data Analysis Workshop (CDAW), "Do all CMEs have flux ropes?", by using a qualitative helicity sign comparison between interplanetary CMEs (ICMEs) and their CME source regions. For this, we select 34 CME-ICME pairs whose source active regions (ARs) have continuous SOHO/MDI magnetogram data covering more than 24 hr without data gap during the passage of the ARs near the solar disk center. The helicity signs in the ARs are determined by estimation of cumulative magnetic helicity injected through the photosphere in the entire source ARs. The helicity signs in the ICMEs are estimated by applying the cylinder model developed by Marubashi (Adv. Space. Res., 26, 55, 2000) to 16 second resolution magnetic field data from the MAG instrument onboard the ACE spacecraft. It is found that 30 out of 34 events (88 %) are helicity sign-consistent events, while four events (12 %) are sign-inconsistent. Through a detailed investigation of the source ARs of the four sign-inconsistent events, we find that those events can be explained by the local helicity sign opposite to that of the entire AR helicity (28 July 2000 ICME), incorrectly reported solar source region in the CDAW list (20 May 2005 ICME), or the helicity sign of the pre-existing coronal magnetic field (13 October 2000 and 20 November 2003 ICMEs). We conclude that the helicity signs of the ICMEs are quite consistent with those of the injected helicities in the AR regions from where the CMEs erupted. C1 [Cho, K. -S.; Park, S. -H.; Marubashi, K.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Cho, K. -S.; Gopalswamy, N.; Akiyama, S.; Yashiro, S.; Kim, R. -S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cho, K. -S.; Akiyama, S.; Yashiro, S.; Kim, R. -S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Lim, E. -K.] New Jersey Inst Technol, Big Bear Solar Observ, Newark, CA USA. RP Cho, KS (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM kscho@kasi.re.kr RI Park, Sung-Hong/K-1578-2014 OI Park, Sung-Hong/0000-0001-9149-6547 FU AFOSR [FA 9550-12-1-0066]; "Development of Korean Space Weather Center" of KASI; KASI basic research funds FX We are grateful to the referee for helpful and constructive comments. SOHO is a project of international cooperation between ESA and NASA. We thank the ACE Science center for the ACE data and to the Yohkoh SXT team and GOES SXI team for the solar X-ray images. This work benefited from the NASA/LWS Coordinated Data Analysis Workshops on CME flux ropes in 2010 and 2011. We acknowledge the workshop support provided by NASA/LWS, Predictive Science, Inc. (San Diego, CA), University of Alcala (Alcala de Henares, Spain), and Ministerio de Ciencia e Innovacion (Reference number AYA2010-1239-E), Spain. E.-K.L. is supported by AFOSR (FA 9550-12-1-0066). K.-S.C. was supported by the "Development of Korean Space Weather Center" of KASI and the KASI basic research funds. NR 44 TC 5 Z9 5 U1 4 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 105 EP 127 DI 10.1007/s11207-013-0224-9 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300008 ER PT J AU Al-Haddad, N Nieves-Chinchilla, T Savani, NP Mostl, C Marubashi, K Hidalgo, MA Roussev, II Poedts, S Farrugia, CJ AF Al-Haddad, N. Nieves-Chinchilla, T. Savani, N. P. Moestl, C. Marubashi, K. Hidalgo, M. A. Roussev, I. I. Poedts, S. Farrugia, C. J. TI Magnetic Field Configuration Models and Reconstruction Methods for Interplanetary Coronal Mass Ejections SO SOLAR PHYSICS LA English DT Article DE Sun: corona; Sun: coronal mass ejections (CMEs) ID STRUCTURED SOLAR-WIND; IN-SITU OBSERVATIONS; FLUX ROPE MODELS; FORCE-FREE FIELD; 1 AU; CONSTANT-ALPHA; CLOUDS; EARTH; SIMULATION; EVOLUTION AB This study aims to provide a reference for different magnetic field models and reconstruction methods for interplanetary coronal mass ejections (ICMEs). To understand the differences in the outputs of these models and codes, we analyzed 59 events from the Coordinated Data Analysis Workshop (CDAW) list, using four different magnetic field models and reconstruction techniques; force-free fitting, magnetostatic reconstruction using a numerical solution to the Grad-Shafranov equation, fitting to a self-similarly expanding cylindrical configuration and elliptical, non-force-free fitting. The resulting parameters of the reconstructions for the 59 events are compared statistically and in selected case studies. The ability of a method to fit or reconstruct an event is found to vary greatly; this depends on whether the event is a magnetic cloud or not. We find that the magnitude of the axial field is relatively consistent across models, but that the axis orientation of the ejecta is not. We also find that there are a few cases with different signs of the magnetic helicity for the same event when we leave the boundaries free to vary, which illustrates that this simplest of parameters is not necessarily always clearly constrained by fitting and reconstruction models. Finally, we examine three unique cases in depth to provide a comprehensive idea of the different aspects of how the fitting and reconstruction codes work. C1 [Al-Haddad, N.; Poedts, S.] Katholieke Univ Leuven, Ctr Plasma Astrofys, B-3001 Heverlee, Belgium. [Nieves-Chinchilla, T.] GSFC NASA, Heliospher Phys Lab, Greenbelt, MD USA. [Nieves-Chinchilla, T.] IACS CUA, Washington, DC USA. [Savani, N. P.] UCAR, Boulder, CO USA. [Savani, N. P.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Moestl, C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Moestl, C.] Graz Univ, Inst Phys, Kanzelhohe Observ, IGAM, A-8010 Graz, Austria. [Marubashi, K.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hidalgo, M. A.] SRG UAH, Madrid, Spain. [Roussev, I. I.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Farrugia, C. J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Farrugia, C. J.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. RP Al-Haddad, N (reprint author), Katholieke Univ Leuven, Ctr Plasma Astrofys, Celestijnenlaan 200B, B-3001 Heverlee, Belgium. EM nada.alhaddad@student.kuleuven.be RI Savani, Neel/G-4066-2014; Nieves-Chinchilla, Teresa/F-3482-2016; Poedts, Stefaan/C-9775-2012; Hidalgo, Miguel/L-5826-2014; OI Savani, Neel/0000-0002-1916-7877; Nieves-Chinchilla, Teresa/0000-0003-0565-4890; Poedts, Stefaan/0000-0002-1743-0651; Hidalgo, Miguel/0000-0003-1617-2037; Moestl, Christian/0000-0001-6868-4152 FU NSF [AGS-0639335]; NASA [NNX10AQ29G, NAS5-0313]; NASA LWS Jack Eddy Postdoctoral Fellowship Program; Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme; European Union Seventh Framework Programme (FP7) [263252] FX N. A. and I. R. were supported by a NSF grant AGS-0639335 (CAREER). This work was initiated at two Coordinated Data Analysis Workshops (CDAWs) held at Predictive Science Inc. in San Diego, CA and at the University of Alcala in Alcala de Henares, Spain with support from NASA and from Spain. N. P. S. was supported by the NASA LWS Jack Eddy Postdoctoral Fellowship Program, administrated by the UCAR Visiting Scientist Program and hosted by the Naval Research Laboratory. C. M. was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. The presented work has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no 263252 [COMESEP]. C. J. F. acknowledges support from NASA grant NNX10AQ29G and NAS5-0313. N. A. would like to thank the Space Science Center at the University of New Hampshire for providing a nice work environment during the final revisions of this manuscript. NR 82 TC 12 Z9 12 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 129 EP 149 DI 10.1007/s11207-013-0244-5 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300009 ER PT J AU Riley, P Richardson, IG AF Riley, P. Richardson, I. G. TI Using Statistical Multivariable Models to Understand the Relationship Between Interplanetary Coronal Mass Ejecta and Magnetic Flux Ropes SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections; Magnetic flux ropes; Magnetic clouds ID IN-SITU SIGNATURES; SOLAR-WIND; CLOUDS; SPACECRAFT; SIMULATION; LOCATIONS; HELIOS; SHOCKS AB In-situ measurements of interplanetary coronal mass ejections (ICMEs) display a wide range of properties. A distinct subset, "magnetic clouds" (MCs), are readily identifiable by a smooth rotation in an enhanced magnetic field, together with an unusually low solar wind proton temperature. In this study, we analyze Ulysses spacecraft measurements to systematically investigate five possible explanations for why some ICMEs are observed to be MCs and others are not: i) An observational selection effect; that is, all ICMEs do in fact contain MCs, but the trajectory of the spacecraft through the ICME determines whether the MC is actually encountered; ii) interactions of an erupting flux rope (FR) with itself or between neighboring FRs, which produce complex structures in which the coherent magnetic structure has been destroyed; iii) an evolutionary process, such as relaxation to a low plasma-beta state that leads to the formation of an MC; iv) the existence of two (or more) intrinsic initiation mechanisms, some of which produce MCs and some that do not; or v) MCs are just an easily identifiable limit in an otherwise continuous spectrum of structures. We apply quantitative statistical models to assess these ideas. In particular, we use the Akaike information criterion (AIC) to rank the candidate models and a Gaussian mixture model (GMM) to uncover any intrinsic clustering of the data. Using a logistic regression, we find that plasma-beta, CME width, and the ratio O (7)/O (6) are the most significant predictor variables for the presence of an MC. Moreover, the propensity for an event to be identified as an MC decreases with heliocentric distance. These results tend to refute ideas ii) and iii). GMM clustering analysis further identifies three distinct groups of ICMEs; two of which match (at the 86 % level) with events independently identified as MCs, and a third that matches with non-MCs (68 % overlap). Thus, idea v) is not supported. Choosing between ideas i) and iv) is more challenging, since they may effectively be indistinguishable from one another by a single in-situ spacecraft. We offer some suggestions on how future studies may address this. C1 [Riley, P.] Predict Sci Inc, San Diego, CA USA. [Richardson, I. G.] NASA Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD USA. [Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Riley, P (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA USA. EM pete@predsci.com; ian.g.richardson@nasa.gov OI Riley, Pete/0000-0002-1859-456X; Richardson, Ian/0000-0002-3855-3634 FU NSF's FESD program; NASA SRT program; NASA GI program; NRL FX P.R. gratefully acknowledges the support of NSF's FESD program as well as NASA SR&T and GI programs, the latter through a subcontract with NRL. We also acknowledge the use of Ulysses observations from NASA/GSFC's Space Physics Data Facility's COHOWeb service, and thank the Ulysses PIs who have made their observations available via this source. NR 44 TC 10 Z9 10 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 217 EP 233 DI 10.1007/s11207-012-0006-9 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300014 ER PT J AU Osherovich, V Fainberg, J Webb, A AF Osherovich, Vladimir Fainberg, Joseph Webb, Alla TI Observational Evidence for a Double-Helix Structure in CMEs and Magnetic Clouds SO SOLAR PHYSICS LA English DT Article DE Quasi-invariant; Solar wind; Magnetic clouds; Coronal mass ejections ID WIND QUASI-INVARIANT; EIGENVALUE SOLUTIONS; FLUX ROPE; EQUILIBRIUM; FIELD; MODEL; FILAMENTS; INDEX AB We compare recent observations of a solar eruptive prominence as seen in extreme-UV light on 30 March 2010 by the Solar Dynamics Observatory (SDO) with the multi-tube model for interplanetary magnetic clouds (Osherovich, Fainberg, Stone, Geophys. Res. Lett. 26, 2597, 1999). Our model is based on an exact analytical solution of the plasma equilibrium with magnetic force balanced by a gradient of scalar gas pressure. Topologically, this solution describes two magnetic helices with opposite magnetic polarity embedded in a cylindrical magnetic flux tube that creates magnetic flux inequality between the two helices by enhancing one helix and suppressing the other. The magnetic field in this model is continuous everywhere and has a finite magnetic energy per unit length of the tube. These configurations have been introduced as MHD bounded states (Osherovich, Soln. Dannye 5, 70, 1975). Apparently, the SDO observations depict two non-equal magnetically interacting helices described by this analytical model. We consider magnetic and thermodynamic signatures of multiple magnetic flux ropes inside the same magnetic cloud, using in situ observations. The ratio of magnetic energy density to bulk speed solar wind energy density has been defined as a solar wind quasi-invariant (QI). We analyze the structure of the QI profile to probe the topology of the internal structure of magnetic clouds. From the superposition of 12 magnetically isolated clouds observed by Ulysses, we have found that the corresponding QI is consistent with our double helix model. C1 [Osherovich, Vladimir] NASA, Goddard Space Flight Ctr, CUA, Greenbelt, MD 20771 USA. [Fainberg, Joseph] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Webb, Alla] Montgomery Coll, Rockville, MD 20850 USA. RP Fainberg, J (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA. EM vladimir.osherovich@gmail.com; fainberg@jhu.edu; allawebb@gmail.com NR 38 TC 0 Z9 0 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 261 EP 274 DI 10.1007/s11207-013-0278-8 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300017 ER PT J AU Hu, Q Farrugia, CJ Osherovich, VA Mostl, C Szabo, A Ogilvie, KW Lepping, RP AF Hu, Qiang Farrugia, C. J. Osherovich, V. A. Mostl, C. Szabo, A. Ogilvie, K. W. Lepping, R. P. TI Effect of Electron Pressure on the Grad-Shafranov Reconstruction of Interplanetary Coronal Mass Ejections SO SOLAR PHYSICS LA English DT Article DE ICMEs; Magnetic clouds; Flux rope; Electron temperature; Grad-Shafranov reconstruction ID IN-SITU OBSERVATIONS; MAGNETIC CLOUD; SOLAR-WIND; MAGNETOPAUSE STRUCTURES; FLUX ROPES; CLUSTER; AU; RECONNECTION; SPACECRAFT; REGION AB We investigate the effect of electron pressure on the Grad-Shafranov (GS) reconstruction of Interplanetary Coronal Mass Ejection (ICME) structures. The GS method uses in situ magnetic field and plasma measurements to solve for a magnetohydrostatic quasi-equilibrium state of space plasmas. For some events, a magnetic flux-rope structure embedded within the ICME can be reconstructed. The electron temperature contributes directly to the calculation of the total plasma pressure, and in ICMEs its contribution often substantially exceeds that of proton temperature. We selected ICME events observed with the Wind spacecraft at 1 AU and applied the GS reconstruction method to each event for cases with and without electron temperature measurements. We sorted them according to the proton plasma beta (the ratio of proton plasma pressure to magnetic pressure) and the electron-to-proton temperature ratio. We present case studies of three representative events, show the cross sections of GS reconstructed flux-rope structure, and discuss the electron pressure contribution to key quantities in the numerical reconstruction procedure. We summarize and compare the geometrical and physical parameters derived from the GS reconstruction results for cases with and without electron temperature contribution. We conclude that overall the electron pressure effect on the GS reconstruction results contributes to a 10 -aEuro parts per thousand 20 % discrepancy in some key physical quantities, such as the magnetic flux content of the ICME flux rope observed at 1 AU. C1 [Hu, Qiang] Univ Alabama, Dept Phys, CSPAR, Huntsville, AL 35899 USA. [Farrugia, C. J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Osherovich, V. A.; Szabo, A.; Ogilvie, K. W.; Lepping, R. P.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Mostl, C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Mostl, C.] Graz Univ, Inst Phys, IGAM, Kanzelhohe Observ, Graz, Austria. RP Hu, Q (reprint author), Univ Alabama, Dept Phys, CSPAR, Huntsville, AL 35899 USA. EM qh0001@uah.edu; charlie.farrugia@unh.edu OI Moestl, Christian/0000-0001-6868-4152 FU NASA [NNG06GD41G, NNX10AQ29G, NNX12AF97G, NNX12AH50G]; NSF [AGS-1140211]; NSF SHINE [AGS-1062050]; European Union Seventh Framework Programme (FP7) [263252]; Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme FX HQ and CJF acknowledge NASA grant NNG06GD41G for partial support. Work at UNH was also supported by NASA Wind grant NNX10AQ29G and NSF grant AGS-1140211. HQ is also grateful for partial support from NASA grants NNX12AF97G and NNX12AH50G, and NSF SHINE AGS-1062050. CM acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no 263252 [COMESEP]. This research was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. We are grateful to NASA CDAWeb for the Wind spacecraft data. NR 43 TC 9 Z9 9 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAY PY 2013 VL 284 IS 1 BP 275 EP 291 DI 10.1007/s11207-013-0259-y PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133ZL UT WOS:000318179300018 ER PT J AU Dreyer, CB Zacny, K Steele, JPH Schwendeman, JR Paulsen, G Andersen, RC Skok, J AF Dreyer, Christopher B. Zacny, Kris Steele, John P. H. Schwendeman, James R. Paulsen, Gale Andersen, Robert C. Skok, John TI Development of a thin section device for space exploration: Overview and system performance estimates SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Planetary missions; In situ measurement; Sample preparation; Space science instrument ID SPECTROMETER AB In this paper we present a conceptual design of a spaceborne instrument for the in situ production of rock thin sections on planetary surfaces. The in situ Automated Rock Thin Section Instrument (IS-ARTS) conceptual design demonstrates that the in situ production of thin sections on a planetary body is a plausible new instrument capability for future planetary exploration. Thin section analysis would reduce much ambiguity in the geological history of a sampled site that is present with instruments currently flown. The technical challenge of producing a thin section device compatible with the spacecraft environment is formidable and has been thought too technically difficult to be practical. Terrestrial thin section preparation requires a skilled petrographist, several preparation instruments that individually exceed typical spacecraft mass and power limits, and consumable materials that are not easily compatible with spaceflight. In two companion papers we present research and development work used to constrain the capabilities of IS-ARTS in the technical space compatible with the spacecraft environment. For the design configuration shown we conclude that a device can be constructed that is capable of 50 sample preparations over a 2 year lifespan with mass, power, and volume constraints compatible with current landed Mars mission configurations. The technical requirements of IS-ARTS (mass, power and number of samples produced) depend strongly on the sample mechanical properties, sample processing rate, the sample size and number of samples to be produced. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Dreyer, Christopher B.; Steele, John P. H.; Schwendeman, James R.; Skok, John] Colorado Sch Mines, Golden, CO 80401 USA. [Zacny, Kris; Paulsen, Gale] Honeybee Robot Spacecraft Mech Corp, Pasadena, CA 91101 USA. [Andersen, Robert C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dreyer, CB (reprint author), Colorado Sch Mines, 1600 Illinois St, Golden, CO 80401 USA. EM cdreyer@mines.edu; zacny@honey-beerobotics.com; jsteele@mines.edu; jim.sch-wendeman@gmail.com; paulsen@honeybeerobotics.com; robert.c.anderson@jpl.nasa.gov; jskok@mines.edu FU NASA Planetary Instrument Definition and Development program [NNX06AH15G] FX This work was funded by NASA Planetary Instrument Definition and Development program (contract # NNX06AH15G). We would like to thank Douglas Stoeser and Steve Wilson from United Sates Geological Survey and Douglas Rickman of NASA Marshall Space Flight Center for providing rock samples. We also would like to acknowledge Attila Szucs of Advanced Superabrasives Inc. for his advice and dedication to this effort and providing grinding and polishing wheels. We also thank John Hodsden from Diamond Wire Technologies for advice on wire saw design. NR 19 TC 2 Z9 2 U1 1 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 1 PY 2013 VL 51 IS 9 BP 1659 EP 1673 DI 10.1016/j.asr.2012.12.012 PG 15 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 129YB UT WOS:000317878800008 ER PT J AU Joshi, RP Qiu, H Tripathi, RK AF Joshi, Ravindra P. Qiu, Hao Tripathi, Ram K. TI Evaluation of a combined electrostatic and magnetostatic configuration for active space-radiation shielding SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Radiation; Shielding; Electrostatic; Magnetostatic; Deep-space ID MAGNETIC-FIELD; PROTECTION AB Developing successful and optimal solutions to mitigating the hazards of severe space radiation in deep space long duration missions is critical for the success of deep-space explorations. A recent report (Tripathi et al., 2008) had explored the feasibility of using electrostatic shielding. Here, we continue to extend the electrostatic shielding strategy and examine a hybrid configuration that utilizes both electrostatic and magnetostatic fields. The main advantages of this system are shown to be: (i) a much better shielding and repulsion of incident ions from both solar particle events (SPE) and galactic cosmic rays (GCR), (ii) reductions in the power requirement for re-charging the electrostatic sub-system, and (iii) low requirements of the magnetic fields that are well below the thresholds set for health and safety for long-term exposures. Furthermore, our results show transmission levels reduced to levels as low as 30% for energies around 1000 MeV, and near total elimination of SPE radiation by these hybrid configurations. It is also shown that the power needed to replenish the electrostatic charges due to particle hits from the GCR and SPE radiation is minimal. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Joshi, Ravindra P.; Qiu, Hao] Old Dominion Univ, Dept Elect & Comp Engn, Norfolk, VA 23529 USA. [Tripathi, Ram K.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Joshi, RP (reprint author), Old Dominion Univ, Dept Elect & Comp Engn, Norfolk, VA 23529 USA. EM rjoshi@odu.edu FU NASA Innovative Advanced Concept (NIAC) Program; NASA Langley Research Center [NNX11AG71G] FX This work was supported in part by NASA Innovative Advanced Concept (NIAC) Program. The team at Old Dominion University (RPJ and HQ) acknowledges the NASA Langley Research Center for partial support through grant No. NNX11AG71G. Useful discussions with Prof. G. Flandro's group (Univ. Tennessee Space Institute) are also greatly appreciated. NR 28 TC 0 Z9 0 U1 6 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 1 PY 2013 VL 51 IS 9 BP 1784 EP 1791 DI 10.1016/j.asr.2012.12.016 PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 129YB UT WOS:000317878800019 ER PT J AU Walker, SA Townsend, LW Norbury, JW AF Walker, Steven A. Townsend, Lawrence W. Norbury, John W. TI Heavy ion contributions to organ dose equivalent for the 1977 galactic cosmic ray spectrum SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Galactic cosmic rays; Space radiation ID INTERPLANETARY MISSIONS; RADIATION PROTECTION; EXPOSURES; DOSIMETRY; HZETRN AB Estimates of organ dose equivalents for the skin, eye lens, blood forming organs, central nervous system, and heart of female astronauts from exposures to the 1977 solar minimum galactic cosmic radiation spectrum for various shielding geometries involving simple spheres and locations within the Space Transportation System (space shuttle) and the International Space Station (ISS) are made using the HZETRN 2010 space radiation transport code. The dose equivalent contributions are broken down by charge groups in order to better understand the sources of the exposures to these organs. For thin shields, contributions from ions heavier than alpha particles comprise at least half of the organ dose equivalent. For thick shields, such as the ISS locations, heavy ions contribute less than 30% and in some cases less than 10% of the organ dose equivalent. Secondary neutron production contributions in thick shields also tend to be as large, or larger, than the heavy ion contributions to the organ dose equivalents. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Walker, Steven A.] Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. [Townsend, Lawrence W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Norbury, John W.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Norbury, JW (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. EM steven.a.walker@nasa.gov; ltownsen@utk.edu; john.w.norbury@nasa.gov FU NASA [NNX09AR20A, NNX10A-D18A] FX The authors thank Francis Badavi, Steve Blattnig, Martha Clowdsley and Jonathan Ransom for reviewing the manuscript. This work was supported by NASA Grants NNX09AR20A (Old Dominion University) and NNX10A-D18A (University of Tennessee). NR 28 TC 7 Z9 7 U1 0 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 1 PY 2013 VL 51 IS 9 BP 1792 EP 1799 DI 10.1016/j.asr.2012.12.011 PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 129YB UT WOS:000317878800020 ER PT J AU Hosamani, R Muralidhara AF Hosamani, Ravikumar Muralidhara TI ACUTE EXPOSURE OF Drosophila melanogaster TO PARAQUAT CAUSES OXIDATIVE STRESS AND MITOCHONDRIAL DYSFUNCTION SO ARCHIVES OF INSECT BIOCHEMISTRY AND PHYSIOLOGY LA English DT Article DE Drosophila; oxidative stress; paraquat; mitochondrial dysfunction ID ENVIRONMENTAL RISK-FACTORS; SPORADIC PARKINSONS-DISEASE; LIFE-SPAN; RESISTANCE; GLUTATHIONE; ROTENONE; NEURODEGENERATION; CATALASE; MODELS; CELLS AB Paraquat (PQ; 1, 1-dimethyl-4-4-bipyridinium), an herbicide and model neurotoxicant, is identified to be one of the prime risk factors in Parkinson's disease (PD). In the Drosophila system, PQ is commonly used to measure acquired resistance against oxidative stress (PQ resistance test). Despite this, under acute PQ exposure, data on the oxidative stress response and associated impact on mitochondria among flies is limited. Accordingly, in this study, we measured markers of oxidative stress and mitochondrial dysfunctions among adult male flies (810 days old) exposed to varying concentrations of PQ (10, 20, and 40 mM in 5% sucrose solution) employing a conventional filter disc method for 24 h. PQ exposure resulted in significant elevation in the levels of oxidative stress biomarkers (malondialdehyde: 43% increase: hydroperoxide: 3239% increase), with concomitant enhancement in reduced glutathione and total thiol levels in cytosol. Higher activity of antioxidant enzymes were also evident along with increased free iron levels. Furthermore, PQ exposure caused a concentration-dependent increase in mitochondrial superoxide generation and activity of manganese-superoxide dismutase (Mn-SOD). The activity levels of complex I-III, complex II-III, and Mg+2 adinosine triphosphatase (ATPase) were also decreased significantly. A robust diminution in the activity of succinate dehydrogenase and moderate decline in the citrate synthase activity suggested a specific effect on citric acid cycle enzymes. Collectively, these data suggest that acute PQ exposure causes significant oxidative stress and mitochondrial dysfunction among flies in vivo. It is suggested that in various experimental settings, while conducting the PQ resistance stress test incorporation of selected biochemical end points is likely to enhance the quality of the data. C1 [Hosamani, Ravikumar; Muralidhara] CSIR, Cent Food Technol Res Inst, Dept Biochem & Nutr, Mysore, Karnataka, India. [Hosamani, Ravikumar] NASA, Space Biosci Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hosamani, R (reprint author), NASA, Space Biosci Div, Ames Res Ctr, Moffett Field, CA 94035 USA. EM ravikumarh82@gmail.com FU University Grant Commission (UGC), India FX We thank the Director of CFTRI for his encouragement in this study. The first author (R. Hosamani) thanks the University Grant Commission (UGC), India, for the award of Junior and Senior Research Fellowships. NR 50 TC 20 Z9 21 U1 2 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0739-4462 J9 ARCH INSECT BIOCHEM JI Arch. Insect Biochem. Physiol. PD MAY PY 2013 VL 83 IS 1 BP 25 EP 40 DI 10.1002/arch.21094 PG 16 WC Biochemistry & Molecular Biology; Entomology; Physiology SC Biochemistry & Molecular Biology; Entomology; Physiology GA 129RY UT WOS:000317860800004 PM 23564607 ER PT J AU Li, D Kauffmann, J Zhang, Q Chen, W AF Li, D. Kauffmann, J. Zhang, Q. Chen, W. TI MASSIVE QUIESCENT CORES IN ORION: DYNAMICAL STATE REVEALED BY HIGH-RESOLUTION AMMONIA MAPS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instrumentation: interferometers; ISM: clouds; ISM: individual objects (Orion); stars: formation Online-only material: color figures ID MOLECULAR CLOUDS; DENSE CORES; DARK CLOUDS; PROTOSTELLAR CORES; INITIAL CONDITIONS; KINEMATICS; OUTFLOWS; CLUSTERS; SHAPES; STARS AB We present combined Very Large Array and Green Bank Telescope images of NH3 inversion transitions (1, 1) and (2, 2) toward OMC2 and OMC3. We focus on the relatively quiescent Orion cores, which are away from the Trapezium cluster and have no sign of massive protostars or evolved star formation. The 5 '' angular resolution and 0.6kms(-1) velocity resolution enable us to study the thermal and dynamic state of these cores at similar to 0.02 pc scales, comparable to or smaller than those of the current dust continuum surveys. We measure temperatures for a total of 30 cores, with average masses of 11 M-circle dot, radii of 0.039 pc, virial mass ratio (R-vir) over bar = 3.9, and critical mass ratio (R-C) over bar = 1.5. Twelve sources contain Spitzer protostars. The thus defined starless and protostellar subsamples have similar temperature, line width, but different masses, with an average of 7.3 M-circle dot for the former and 16 M-circle dot for the latter. Compared to other Gould Belt dense cores, more Orion cores have a high gravitational-to-kinetic energy ratio and more cores have a larger than unity critical mass ratio. Orion dense cores have velocity dispersions similar to those of cores in low-mass star-forming regions but larger masses for given size. Some cores appear to have truly supercritical gravitational-to-kinetic energy ratios, even when considering significant observational uncertainties: thermal and non-thermal gas motions alone cannot prevent collapse. C1 [Li, D.] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China. [Li, D.] Space Sci Inst, Boulder, CO USA. [Li, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Kauffmann, J.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chen, W.] Peking Univ, Beijing 100871, Peoples R China. RP Li, D (reprint author), Chinese Acad Sci, Natl Astron Observ, Chaoyang Dist Datun Rd A20, Beijing, Peoples R China. EM ithaca.li@gmail.com OI Zhang, Qizhou/0000-0003-2384-6589 NR 37 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 1 PY 2013 VL 768 IS 1 AR L5 DI 10.1088/2041-8205/768/1/L5 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130KD UT WOS:000317912900005 ER PT J AU Finke, N Hoehler, TM Polerecky, L Buehring, B Thamdrup, B AF Finke, Niko Hoehler, Tori M. Polerecky, Lubos Buehring, Benjamin Thamdrup, Bo TI Competition for inorganic carbon between oxygenic and anoxygenic phototrophs in a hypersaline microbial mat, Guerrero Negro, Mexico SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID MICROCOLEUS-CHTHONOPLASTES; CYANOBACTERIAL MATS; PHOTOSYNTHESIS; BIOGEOCHEMISTRY; DIVERSITY; BACTERIA; MARINE; SULFUR; LIGHT; ENVIRONMENTS AB While most oxygenic phototrophs harvest light only in the visible range (400700nm, VIS), anoxygenic phototrophs can harvest near infrared light (>700nm, NIR). To study interactions between the photosynthetic guilds we used microsensors to measure oxygen and gross oxygenic photosynthesis (gOP) in a hypersaline microbial mat under full (VIS+NIR) and VIS illumination. Under normal dissolved inorganic carbon (DIC) concentrations (2mM), volumetric rates of gOP were reduced up to 65% and areal rates by 1631% at full compared with VIS illumination. This effect was enhanced (reduction up to 100% in volumetric, 50% in areal rates of gOP) when DIC was lowered to 1mM, but diminished at 10mM DIC or lowered pH. In conclusion, under full-light illumination anoxygenic phototrophs are able to reduce the activity of oxygenic phototrophs by efficiently competing for inorganic carbon within the highly oxygenated layer. Anoxygenic photosynthesis, calculated from the difference in gOP under full and VIS illumination, represented between 10% and 40% of the C-fixation. The DIC depletion in the euphotic zone as well as the significant C-fixation by anoxygenic phototrophs in the oxic layer influences the carbon isotopic composition of the mat, which needs to be taken into account when interpreting isotopic biosignals in geological records. C1 [Finke, Niko; Thamdrup, Bo] Univ Southern Denmark, Inst Biol, Nord Ctr Earth Evolut, Odense, Denmark. [Finke, Niko; Hoehler, Tori M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Polerecky, Lubos] Max Planck Inst Marine Microbiol, Microsensorgrp, Bremen, Germany. [Buehring, Benjamin] Univ Bremen, Marum, D-28359 Bremen, Germany. RP Finke, N (reprint author), Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. EM nfinke@web.de RI Polerecky, Lubos/E-1134-2014; Thamdrup, Bo/F-3889-2016 OI Polerecky, Lubos/0000-0003-4425-585X; Thamdrup, Bo/0000-0002-1221-7077 FU Oak Ridge Postdoctoral Fellowship; Marie Curie Outgoing International Fellowship [22154] FX We thank Brad Bebout for help with the microsensor measurements, Gaby Eickert for help building the scalar irradiance probes, Michael Kuhl for help with the absolute irradiance measurements and Dirk de Beer for fruitful discussion. We also thank three anonymous reviewers whose comments helped improve the manuscript. The work was funded by an Oak Ridge Postdoctoral Fellowship and a Marie Curie Outgoing International Fellowship (Project # 22154). NR 43 TC 6 Z9 6 U1 2 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1462-2912 EI 1462-2920 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD MAY PY 2013 VL 15 IS 5 SI SI BP 1532 EP 1550 DI 10.1111/1462-2920.12032 PG 19 WC Microbiology SC Microbiology GA 132BD UT WOS:000318041800022 PM 23347091 ER PT J AU Canion, A Prakash, O Green, SJ Jahnke, L Kuypers, MMM Kostka, JE AF Canion, Andy Prakash, Om Green, Stefan J. Jahnke, Linda Kuypers, Marcel M. M. Kostka, Joel E. TI Isolation and physiological characterization of psychrophilic denitrifying bacteria from permanently cold Arctic fjord sediments (Svalbard, Norway) SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID 16S RIBOSOMAL-RNA; CENTRAL BALTIC SEA; SP-NOV.; MARINE-SEDIMENTS; COMMUNITY STRUCTURE; TEMPERATURE-DEPENDENCE; SHELF SEDIMENTS; FATTY-ACIDS; DIVERSITY; NITROGEN AB A large proportion of reactive nitrogen loss from polar sediments is mediated by denitrification, but microorganisms mediating denitrification in polar environments remain poorly characterized. A combined approach of most-probable-number (MPN) enumeration, cultivation and physiological characterization was used to describe psychrophilic denitrifying bacterial communities in sediments of three Arctic fjords in Svalbard (Norway). A MPN assay showed the presence of 103106 cells of psychrophilic nitrate-respiring bacteria g1 of sediment. Fifteen strains within the Proteobacteria were isolated using a systematic enrichment approach with organic acids as electron donors and nitrate as an electron acceptor. Isolates belonged to five genera, including Shewanella, Pseudomonas, Psychromonas (Gammaproteobacteria), Arcobacter (Epsilonproteobacteria) and Herminiimonas (Betaproteobacteria). All isolates were denitrifiers, except Shewanella, which exhibited the capacity for dissimilatory nitrate reduction to ammonium (DNRA). Growth from 0 to 40 degrees C demonstrated that all genera except Shewanella were psychrophiles with optimal growth below 15 degrees C, and adaptation to low temperature was demonstrated as a shift from primarily C16:0 saturated fatty acids to C16:1 monounsaturated fatty acids at lower temperatures. This study provides the first targeted enrichment and characterization of psychrophilic denitrifying bacteria from polar sediments, and two genera, Arcobacter and Herminiimonas, are isolated for the first time from permanently cold marine sediments. C1 [Canion, Andy; Prakash, Om] Florida State Univ, Earth Ocean & Atmospher Sci Dept, Tallahassee, FL 32306 USA. [Green, Stefan J.] Univ Illinois, DNA Serv Facil, Chicago, IL USA. [Green, Stefan J.] Univ Illinois, Dept Biol Sci, Chicago, IL 60680 USA. [Jahnke, Linda] NASA, Ames Res Ctr, Astrobiol Inst, Moffett Field, CA 94035 USA. [Kuypers, Marcel M. M.] Max Planck Inst Marine Mikrobiol, D-28359 Bremen, Germany. [Kostka, Joel E.] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. RP Kostka, JE (reprint author), Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. EM joel.kostka@biology.gatech.edu RI Canion, Andy/Q-2397-2015; OI Canion, Andy/0000-0003-1604-7631; Green, Stefan/0000-0003-2781-359X FU Max Planck Society; National Science Foundation FX The authors would like to thank captain Stig Henningsen and the crew of the M/S Farm for their assistance with sample collection, and acknowledge cruise participants of the 2008 MPI Svalbard cruise. We also thank Tom Gihring, Will Overholt, Jonathan Delgardio, John Kaba, Niki Norton, Nicole Roberts and Dave Oliff for field sampling, logistical, and analytical assistance. This study was supported by the Max Planck Society and the National Science Foundation. NR 72 TC 10 Z9 10 U1 6 U2 80 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1462-2912 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD MAY PY 2013 VL 15 IS 5 SI SI BP 1606 EP 1618 DI 10.1111/1462-2920.12110 PG 13 WC Microbiology SC Microbiology GA 132BD UT WOS:000318041800028 PM 23530773 ER PT J AU Suvarna, P Tungare, M Leathersich, JM Agnihotri, P Shahedipour-Sandvik, F Bell, LD Nikzad, S AF Suvarna, Puneet Tungare, Mihir Leathersich, Jeffrey M. Agnihotri, Pratik Shahedipour-Sandvik, F. Bell, L. Douglas Nikzad, Shouleh TI Design and Growth of Visible-Blind and Solar-Blind III-N APDs on Sapphire Substrates SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE avalanche photodiode; solar-blind; AlGaN on sapphire; pulsed MOCVD; ultraviolet photodiode ID SUPERLATTICES AB GaN-based visible-blind and AlGaN-based solar-blind avalanche photodiodes (APDs) have been grown and fabricated on sapphire substrates. The GaN p-i-n APDs show low dark current with high gain. The AlGaN layers for the Al0.55Ga0.45N-based APDs are grown using a newly developed pulsed metalorganic chemical vapor deposition (MOCVD) process, and the material characterization results show excellent material quality. The spectral responsivity of the devices show a bandpass characteristic with cutoffs in the ultraviolet (UV) visible-blind and solar-blind spectrum for GaN- and Al0.55Ga0.45N-based APDs, respectively. C1 [Suvarna, Puneet; Tungare, Mihir; Leathersich, Jeffrey M.; Agnihotri, Pratik; Shahedipour-Sandvik, F.] SUNY Albany, Coll Nanoscale Sci & Engn, Albany, NY 12222 USA. [Bell, L. Douglas; Nikzad, Shouleh] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Suvarna, P (reprint author), SUNY Albany, Coll Nanoscale Sci & Engn, Albany, NY 12222 USA. EM psuvarna@albany.edu FU National Aeronautics and Space Administration (NASA) FX This work is funded by National Aeronautics and Space Administration (NASA) and done in collaboration with Jet Propulsion Laboratory. NR 14 TC 9 Z9 9 U1 1 U2 43 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0361-5235 J9 J ELECTRON MATER JI J. Electron. Mater. PD MAY PY 2013 VL 42 IS 5 BP 854 EP 858 DI 10.1007/s11664-013-2537-8 PG 5 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA 131JD UT WOS:000317988300013 ER PT J AU Odom, B AF Odom, Brian TI Channeling the Past: Politicizing History in Postwar America SO LIBRARY JOURNAL LA English DT Book Review C1 [Odom, Brian] NASA, Marshall Space & Flight Ctr Arch, Huntsville, AL USA. RP Odom, B (reprint author), NASA, Marshall Space & Flight Ctr Arch, Huntsville, AL USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 1 PY 2013 VL 138 IS 8 BP 94 EP 94 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 132IE UT WOS:000318060300128 ER PT J AU Mattox, EM Knox, JC Bardot, DM AF Mattox, E. M. Knox, J. C. Bardot, D. M. TI Carbon dioxide removal system for closed loop atmosphere revitalization, candidate sorbents screening and test results SO ACTA ASTRONAUTICA LA English DT Article DE Carbon dioxide removal; Adsorption; Commercial sorbents; Zeolites AB Due to the difficulty and expense it costs to resupply manned-spacecraft habitats, a goal is to create a closed loop atmosphere revitalization system, in which precious commodities such as oxygen, carbon dioxide, and water are continuously recycled. Our aim is to test other sorbents for their capacity for future spacecraft missions, such as on the Orion spacecraft, or possibly lunar or Mars mission habitats to see if they would be better than the zeolite sorbents on the 4-bed molecular sieve. Some of the materials being tested are currently used for other industry applications. Studying these sorbents for their specific spacecraft application is different from that for applications on earth because in space, there are certain power, mass, and volume limitations that are not as critical on Earth. In manned-spaceflight missions, the sorbents are exposed to a much lower volume fraction of CO2 (0.6% volume CO2) than on Earth. LiLSX was tested for its CO2 capacity in an atmosphere like that of the ISS. Breakthrough tests were run to establish the capacities of these materials at a partial pressure of CO2 that is seen on the ISS. This paper discusses experimental results from benchmark materials, such as results previously obtained from tests on Grade 522, and the forementioned candidate materials for the Carbon Dioxide Removal Assembly (CDRA) system. (c) 2012 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Mattox, E. M.; Bardot, D. M.] Univ Alabama Huntsville, Huntsville, AL USA. [Knox, J. C.] NASA, Marshall Space Flight Ctr, Washington, DC USA. RP Mattox, EM (reprint author), Univ Alabama Huntsville, Huntsville, AL USA. EM emm0001@uah.edu; jim.knox@nasa.gov; dmb0012@uah.edu NR 8 TC 7 Z9 7 U1 3 U2 15 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD MAY-JUN PY 2013 VL 86 BP 39 EP 46 DI 10.1016/j.actaastro.2012.09.019 PG 8 WC Engineering, Aerospace SC Engineering GA 120DD UT WOS:000317150100004 ER PT J AU Grzenia, BJ Tycner, C Jones, CE Rinehart, SA van Belle, GT Sigut, TAA AF Grzenia, B. J. Tycner, C. Jones, C. E. Rinehart, S. A. van Belle, G. T. Sigut, T. A. A. TI MODELING CIRCUMSTELLAR DISKS OF B-TYPE STARS WITH OBSERVATIONS FROM THE PALOMAR TESTBED INTERFEROMETER SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: emission-line, Be; techniques: interferometric ID PROTOTYPE OPTICAL INTERFEROMETER; GAMMA-CASSIOPEIAE; ZETA-TAURI; BINARY NATURE; SHELL STARS; EMISSION; BRIGHT; RATES; VARIABILITY; PARAMETERS AB Geometrical (uniform disk) and numerical models were calculated for a set of B-emission (Be) stars observed with the Palomar Testbed Interferometer (PTI). Physical extents have been estimated for the disks of a total of 15 stars via uniform disk models. Our numerical non-LTE models used parameters for the B0, B2, B5, and B8 spectral classes and following the framework laid by previous studies, we have compared them to infrared K-band interferometric observations taken at PTI. This is the first time such an extensive set of Be stars observed with long-baseline interferometry has been analyzed with self-consistent non-LTE numerical disk models. C1 [Grzenia, B. J.; Tycner, C.] Cent Michigan Univ, Dept Phys, Mt Pleasant, MI 48859 USA. [Grzenia, B. J.; Jones, C. E.; Sigut, T. A. A.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Rinehart, S. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [van Belle, G. T.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Grzenia, BJ (reprint author), Cent Michigan Univ, Dept Phys, Mt Pleasant, MI 48859 USA. FU National Aeronautics and Space Administration [NNX08AQ24A]; Jet Propulsion Laboratory; Caltech; National Aeronautics and Space Administration; Canadian Natural Sciences and Engineering Research Council FX This material is based upon work supported by the National Aeronautics and Space Administration under grant No. NNX08AQ24A. The Palomar Testbed Interferometer is operated by the NASA Exoplanet Science Institute and the PTI collaboration and was constructed with funds from the Jet Propulsion Laboratory, Caltech, as provided by the National Aeronautics and Space Administration. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. B.J.G. acknowledges support from Central Michigan University. This research has made use of services produced by the NASA Exoplanet Science Institute at the California Institute of Technology. This work is supported by the Canadian Natural Sciences and Engineering Research Council through Discovery Grants to T.A.A.S. and C.E.J. NR 57 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2013 VL 145 IS 5 AR 141 DI 10.1088/0004-6256/145/5/141 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122PD UT WOS:000317329100025 ER PT J AU Hosek, MW Blaauw, RC Cooke, WJ Suggs, RM AF Hosek, Matthew W., Jr. Blaauw, Rhiannon C. Cooke, William J. Suggs, Robert M. TI OUTBURST DUST PRODUCTION OF COMET 29P/SCHWASSMANN-WACHMANN 1 SO ASTRONOMICAL JOURNAL LA English DT Article DE comets: individual (29P/Schwassmann-Wachmann 1) ID NARROW-BAND PHOTOMETRY; ENVIRONMENT; P/SCHWASSMANN-WACHMANN-1 AB Multi-aperture photometry of Comet 29P/Schwassmann-Wachmann 1 was conducted on Johnson-Cousins R-band observations spanning 2011 May 1-9 and 2012 June 6-July 3. The comet was observed in outburst on 2011 May 3 and 2012 July 1, during which its brightness increased by 2.2 and 2.1 mag, respectively, as measured through a 10 arcsec aperture. Dust production before and after each outburst is calculated using the parameter Af rho, which is converted to a lower limit on the dust production rate based on dust models and derived nuclear properties from other studies. Both outbursts are accompanied by large increases in dust production, Af rho by a factor of similar to 6.5-7 and dust production rate by a factor of similar to 18-23. In addition, variations in the dust brightness profile of the coma are examined during the events. The profile is observed to steepen significantly at the beginning of each outburst and then slowly return to pre-outburst values, mirroring the behavior of Af rho. The start of an outbound "ripple" of dust in the profile might be observed as the comet returns to its pre-outburst state, although this cannot be confirmed. Using a simple model of the 2011 May 3 outburst, an estimated lower limit of (2.6 +/- 0.7) x 10(8) kg of dust was released during the event. If this is representative of a typical outburst of 29P, then it is estimated that outbursts account for a lower limit of 80(-30)(+20) % of the total material ejected by the comet per year. C1 [Hosek, Matthew W., Jr.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Blaauw, Rhiannon C.; Cooke, William J.; Suggs, Robert M.] NASA, George C Marshall Space Flight Ctr, Meteoroid Environm Off, Huntsville, AL 35812 USA. RP Hosek, MW (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM mwhosek@ifa.hawaii.edu FU Meteoroid Environment Office of Marshall Space Flight Center; NASA Academy Program; Massachusetts Space Grant FX The authors thank Julio Castellano and the entire Cometas-Obs group for sharing their observations of Comet 29P/Schwassmann-Wachmann 1, as well as the staff of New Mexico Skies for their technical support throughout the observations. Hosek thanks the Meteoroid Environment Office of Marshall Space Flight Center, the NASA Academy Program, and the Massachusetts Space Grant for supporting and funding his research. The authors also thank the anonymous reviewer whose comments improved the paper. NR 33 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2013 VL 145 IS 5 AR 122 DI 10.1088/0004-6256/145/5/122 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122PD UT WOS:000317329100006 ER PT J AU Mack, CE Ge, J Deshpande, R Wisniewski, JP Stassun, KG Gaudi, BS Fleming, SW Mahadevan, S Lee, ND Eastman, J Ghezzi, L Hernandez, JIG Femenia, B Ferreira, L de Mello, GP Crepp, JR Sanchez, DM Agol, E Beatty, TG Bizyaev, D Brewington, H Cargile, PA da Costa, LN Esposito, M Ebelke, G Hebb, L Jiang, P Kane, SR Lee, B Maia, MAG Malanushenko, E Malanushenko, V Oravetz, D Paegert, M Pan, KK Prieto, CA Pepper, J Rebolo, R Roy, A Santiago, BX Schneider, DP Simmons, A Siverd, RJ Snedden, S Tofflemire, BM AF Mack, Claude E., III Ge, Jian Deshpande, Rohit Wisniewski, John P. Stassun, Keivan G. Gaudi, B. Scott Fleming, Scott W. Mahadevan, Suvrath Lee, Nathan De Eastman, Jason Ghezzi, Luan Hernandez, Jonay I. Gonzalez Femenia, Bruno Ferreira, Leticia de Mello, Gustavo Porto Crepp, Justin R. Mata Sanchez, Daniel Agol, Eric Beatty, Thomas G. Bizyaev, Dmitry Brewington, Howard Cargile, Phillip A. da Costa, Luiz N. Esposito, Massimiliano Ebelke, Garret Hebb, Leslie Jiang, Peng Kane, Stephen R. Lee, Brian Maia, Marcio A. G. Malanushenko, Elena Malanushenko, Victor Oravetz, Daniel Paegert, Martin Pan, Kaike Allende Prieto, Carlos Pepper, Joshua Rebolo, Rafael Roy, Arpita Santiago, Basilio X. Schneider, Donald P. Simmons, Audrey Siverd, Robert J. Snedden, Stephanie Tofflemire, Benjamin M. TI A CAUTIONARY TALE: MARVELS BROWN DWARF CANDIDATE REVEALS ITSELF TO BE A VERY LONG PERIOD, HIGHLY ECCENTRIC SPECTROSCOPIC STELLAR BINARY SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: spectroscopic; brown dwarfs; stars: individual (TYC 3010-1494-1) ID FIXED-DELAY INTERFEROMETER; HOBBY-EBERLY TELESCOPE; LOW-MASS STELLAR; SOLAR-LIKE STARS; EXTERNALLY DISPERSED INTERFEROMETER; SUBSTELLAR COMPANIONS; THEORETICAL ISOCHRONES; LUMINOSITY-RELATION; RADIAL-VELOCITIES; ACCURATE MASSES AB We report the discovery of a highly eccentric, double-lined spectroscopic binary star system (TYC 3010-1494-1), comprising two solar-type stars that we had initially identified as a single star with a brown dwarf companion. At the moderate resolving power of the MARVELS spectrograph and the spectrographs used for subsequent radial-velocity (RV) measurements (R less than or similar to 30,000), this particular stellar binary mimics a single-lined binary with an RV signal that would be induced by a brown dwarf companion (M sin i similar to 50 M-Jup) to a solar-type primary. At least three properties of this system allow it to masquerade as a single star with a very-low-mass companion: its large eccentricity (e similar to 0.8), its relatively long period (P similar to 238 days), and the approximately perpendicular orientation of the semi-major axis with respect to the line of sight (omega similar to 189 degrees). As a result of these properties, for similar to 95% of the orbit the two sets of stellar spectral lines are completely blended, and the RV measurements based on centroiding on the apparently single-lined spectrum is very well fit by an orbit solution indicative of a brown dwarf companion on a more circular orbit (e similar to 0.3). Only during the similar to 5% of the orbit near periastron passage does the true, double-lined nature and large RV amplitude of similar to 15 km s(-1) reveal itself. The discovery of this binary system is an important lesson for RV surveys searching for substellar companions; at a given resolution and observing cadence, a survey will be susceptible to these kinds of astrophysical false positives for a range of orbital parameters. Finally, for surveys like MARVELS that lack the resolution for a useful line bisector analysis, it is imperative to monitor the peak of the cross-correlation function for suspicious changes in width or shape, so that such false positives can be flagged during the candidate vetting process. C1 [Mack, Claude E., III; Stassun, Keivan G.; Lee, Nathan De; Hebb, Leslie; Pepper, Joshua] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Ge, Jian; Fleming, Scott W.; Lee, Nathan De; Jiang, Peng; Lee, Brian] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Deshpande, Rohit; Fleming, Scott W.; Mahadevan, Suvrath; Roy, Arpita; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Deshpande, Rohit; Fleming, Scott W.; Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Wisniewski, John P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN USA. [Gaudi, B. Scott; Eastman, Jason; Beatty, Thomas G.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Ghezzi, Luan; da Costa, Luiz N.; Maia, Marcio A. G.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Ferreira, Leticia; de Mello, Gustavo Porto; da Costa, Luiz N.; Maia, Marcio A. G.; Santiago, Basilio X.] Lab Interinst Eastron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Hernandez, Jonay I. Gonzalez; Mata Sanchez, Daniel; Esposito, Massimiliano; Allende Prieto, Carlos; Rebolo, Rafael] IAC, E-38205 Tenerife, Spain. [Hernandez, Jonay I. Gonzalez; Femenia, Bruno; Mata Sanchez, Daniel; Esposito, Massimiliano; Allende Prieto, Carlos; Rebolo, Rafael] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Ferreira, Leticia; de Mello, Gustavo Porto] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, RJ, Brazil. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Hebb, Leslie] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Bizyaev, Dmitry; Brewington, Howard; Ebelke, Garret; Malanushenko, Elena; Malanushenko, Victor; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA. [Kane, Stephen R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Santiago, Basilio X.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Tofflemire, Benjamin M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Mack, CE (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. EM claude.e.mack@vanderbilt.edu OI Eastman, Jason/0000-0003-3773-5142; Fleming, Scott/0000-0003-0556-027X; Mata Sanchez, Daniel/0000-0003-0245-9424; Roy, Arpita/0000-0001-8127-5775; /0000-0002-0802-9145; Pepper, Joshua/0000-0002-3827-8417 FU Vanderbilt Initiative in Data-Intensive Astrophysics (VIDA); NSF [AST 0349075, AST 0645416, AST-1056524, AST-0705139]; NSF AAPF AST [08-02230]; CNPq [476909/2006-6]; FAPERJ [APQ1/26/170.687/2004]; PAPDRJ CAPES/FAPERJ Fellowship; W. M. Keck Foundation; SDSS-III consortium; NASA [NNX07AP14G]; University of Florida; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; Robert Martin Ayers Sciences Fund; National Aeronautics and Space Administration; National Science Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; French Participation Group; German Participation Group; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; New Mexico State University; New York University; Ohio State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX This research was partially supported by the Vanderbilt Initiative in Data-Intensive Astrophysics (VIDA) and NSF CAREER grant AST 0349075 (C. E. M., K. G. S., L. H., J.P.), NSF AAPF AST 08-02230 (J.P. W.), NSF CAREER grant AST 0645416 (E. A.), CNPq grant 476909/2006-6 (G. F. P. M.), FAPERJ grant APQ1/26/170.687/2004 (G. F. P. M.), NSF CAREER grant AST-1056524 (B. S. G., J.D.E.), and a PAPDRJ CAPES/FAPERJ Fellowship (L.G.).; Based on observations with the SDSS 2.5 m telescope. Funding for the MARVELS multi-object Doppler instrument was provided by the W. M. Keck Foundation and NSF grant AST-0705139. The MARVELS survey was partially funded by the SDSS-III consortium, NSF grant AST-0705139, NASA with grant NNX07AP14G and the University of Florida. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium.; This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund. It also made use of the IRAF software distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. We also make use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 71 TC 7 Z9 7 U1 2 U2 17 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 MAY PY 2013 VL 145 IS 5 AR 139 DI 10.1088/0004-6256/145/5/139 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122PD UT WOS:000317329100023 ER PT J AU Williams, KA Howell, SB Liebert, J Smith, PS Bellini, A Rubin, KHR Bolte, M AF Williams, Kurtis A. Howell, Steve B. Liebert, James Smith, Paul S. Bellini, Andrea Rubin, Kate H. R. Bolte, Michael TI TIME-RESOLVED SPECTROSCOPY OF THE POLAR EU CANCRI IN THE OPEN CLUSTER MESSIER 67 SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; novae, cataclysmic variables; open clusters and associations: individual (Messier 67); stars: individual (EU Cnc); white dwarfs ID CLOSE BINARY-SYSTEM; FINAL MASS RELATION; DA WHITE-DWARFS; CATACLYSMIC VARIABLES; GLOBULAR-CLUSTER; SURROUNDING FIELD; EXTENSIVE SEARCH; CCD PHOTOMETRY; STAR-CLUSTERS; M67 AB We present time-resolved spectroscopic and polarimetric observations of the AM Her system EU Cnc. EU Cnc is located near the core of the old open cluster Messier 67; new proper motion measurements indicate that EU Cnc is indeed a member of the star cluster, and this system therefore is useful to constrain the formation and evolution of magnetic cataclysmic variables. The spectra exhibit two-component emission features with independent radial velocity variations as well as time-variable cyclotron emission indicating a magnetic field strength of 41 MG. The period of the radial velocity and cyclotron hump variations are consistent with the previously known photometric period, and the spectroscopic flux variations are consistent in amplitude with previous photometric amplitude measurements. The secondary star is also detected in the spectrum. We also present polarimetric imaging measurements of EU Cnc that show a clear detection of polarization, and the degree of polarization drops below our detection threshold at phases when the cyclotron emission features are fading or not evident. The combined data are all consistent with the interpretation that EU Cnc is a low-state polar in the cluster Messier 67. The mass function of the system gives an estimate of the accretor mass of M-WD >= 0.68 M-circle dot with M-WD approximate to 0.83 M-circle dot for an average inclination. We are thus able to place a lower limit on the progenitor mass of the accreting white dwarf of >= 1.43 M-circle dot. C1 [Williams, Kurtis A.] Texas A&M Univ, Dept Phys & Astron, Commerce, TX 75429 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Liebert, James; Smith, Paul S.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Bellini, Andrea] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Rubin, Kate H. R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bolte, Michael] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Williams, KA (reprint author), Texas A&M Univ, Dept Phys & Astron, POB 3011, Commerce, TX 75429 USA. EM kurtis.williams@tamuc.edu; steve.b.howell@nasa.gov; jamesliebert@gmail.com; psmith@as.arizona.edu; bellini@stsci.edu; rubin@mpia.de; bolte@ucolick.org OI Williams, Kurtis/0000-0002-1413-7679 FU National Science Foundation [AST-0397492, AST-0602288]; W. M. Keck Foundation FX K.A.W. is grateful for the financial support of National Science Foundation awards AST-0397492 and AST-0602288. The authors thank S. Kafka for discussions on this system and for providing the original data from Nair et al. (2005). We also thank G. Schmidt for providing time from his observing run to obtain the polarimetry in this paper, D. Wickramasinghe for assistance in measuring the magnetic field strength, and the anonymous referee for suggestions leading to improvement of this paper. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 55 TC 3 Z9 3 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2013 VL 145 IS 5 AR 129 DI 10.1088/0004-6256/145/5/129 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122PD UT WOS:000317329100013 ER PT J AU Goodman, SJ Blakeslee, RJ Koshak, WJ Mach, D Bailey, J Buechler, D Carey, L Schultz, C Bateman, M McCaul, E Stano, G AF Goodman, Steven J. Blakeslee, Richard J. Koshak, William J. Mach, Douglas Bailey, Jeffrey Buechler, Dennis Carey, Larry Schultz, Chris Bateman, Monte McCaul, Eugene, Jr. Stano, Geoffrey TI The GOES-R Geostationary Lightning Mapper (GLM) SO ATMOSPHERIC RESEARCH LA English DT Article DE Lightning; Thunderstorms; Satellite meteorology; Nowcasting ID DATA ASSIMILATION TECHNIQUE; WRF-ARW MODEL; TROPICAL CYCLONE; FORECAST MODELS; SEVERE WEATHER; UNITED-STATES; WINTER STORM; IMAGER DATA; CLOUD; THUNDERSTORMS AB The Geostationary Operational Environmental Satellite R-series (GOES-R) is the next block of four satellites to follow the existing GOES constellation currently operating over the Western Hemisphere. Advanced spacecraft and instrument technology will support expanded detection of environmental phenomena, resulting in more timely and accurate forecasts and warnings. Advancements over current GOES capabilities include a new capability for total lightning detection (cloud and cloud-to-ground flashes) from the Geostationary Lightning Mapper (GLM), and improved cloud and moisture imagery with the 16-channel Advanced Baseline Imager (ABI). The GLM will map total lightning activity continuously day and night with near-uniform storm-scale spatial resolution of 8 km with a product refresh rate of less than 20 s over the Americas and adjacent oceanic regions in the western hemisphere. This will aid in forecasting severe storms and tornado activity, and convective weather impacts on aviation safety and efficiency. In parallel with the instrument development an Algorithm Working Group (AWG) Lightning Detection Science and Applications Team developed the Level 2 (stroke and flash) algorithms from the Level 1 lightning event (pixel level) data. Proxy data sets used to develop the GLM operational algorithms as well as cal/val performance monitoring tools were derived from the NASA Lightning Imaging Sensor (US) and Optical Transient Detector (OTD) instruments in low Earth orbit, and from ground-based lightning networks and intensive prelaunch field campaigns. The GLM will produce the same or similar lightning flash attributes provided by the LIS and OTD, and thus extend their combined climatology over the western hemisphere into the coming decades. Science and application development along with preoperational product demonstrations and evaluations at NWS forecast offices and NOAA testbeds will prepare the forecasters to use GLM as soon as possible after the planned launch and checkout of GOES-R in late 2015. New applications will use GLM alone, in combination with the ABI, or integrated (fused) with other available tools (weather radar and ground strike networks, nowcasting systems, mesoscale analysis, and numerical weather prediction models) in the hands of the forecaster responsible for issuing more timely and accurate forecasts and warnings. Published by Elsevier B.V. C1 [Goodman, Steven J.] NOAA, NESDIS GSFC, Greenbelt, MD USA. [Blakeslee, Richard J.; Koshak, William J.] NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35812 USA. [Mach, Douglas; Bailey, Jeffrey; Buechler, Dennis; Carey, Larry; Schultz, Chris] Univ Alabama, Huntsville, AL 35899 USA. [Bateman, Monte; McCaul, Eugene, Jr.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Stano, Geoffrey] ENSCO Inc, Huntsville, AL USA. RP Goodman, SJ (reprint author), NOAA, NESDIS GSFC, Greenbelt, MD USA. EM steven.j.goodman@noaa.gov NR 47 TC 55 Z9 56 U1 1 U2 40 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD MAY PY 2013 VL 125 BP 34 EP 49 DI 10.1016/j.atmosres.2013.01.006 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 127PN UT WOS:000317711000004 ER PT J AU Mills, RD Coleman, DS AF Mills, Ryan D. Coleman, Drew S. TI Temporal and chemical connections between plutons and ignimbrites from the Mount Princeton magmatic center SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY LA English DT Article DE Pluton emplacement; Ignimbrites; Geochronology; Magma flux ID U-PB GEOCHRONOLOGY; JUAN VOLCANIC FIELD; TORRES-DEL-PAINE; RESIDENCE TIMES; NEW-ZEALAND; SIERRA-NEVADA; AR-40/AR-39 CHRONOLOGY; ZIRCON CRYSTALLIZATION; CONTINENTAL-CRUST; DECAY CONSTANTS AB The Mount Princeton magmatic center, located in central Colorado, consists of the epizonal Mount Princeton batholith, the nested Mount Aetna caldera, and volumetrically minor leucogranites. New CA-TIMS U/Pb zircon ages indicate the majority of the Mount Princeton batholith was emplaced during a period of regional ignimbrite quiescence. The structurally highest unit of quartz monzonite yields a Pb-206/U-238 age of 35.80 +/- A 0.10 Ma, and the youngest dated unit of the quartz monzonite is a porphyritic unit that yields a Pb-206/U-238 age of 35.37 +/- A 0.10 Ma. Using the exposed, dated volume of the quartz monzonite and new geochronology yields an estimated pluton filling rate of similar to 0.002 km(3)/a. This rate is comparable to the accumulation rates published for other plutons, and at least an order of magnitude slower than fluxes necessary to support accumulation of large eruptible magma volumes. Geochronology for the two large ignimbrites spatially associated with the batholith indicates a temporal disconnect between the vast majority of pluton building and explosive eruption of magma. The Wall Mountain Tuff erupted from a source in the same geographic area as the Mount Princeton batholith at 37.3 Ma (Ar/Ar sanidine), but no structural evidence of a caldera or temporally associated plutonic rocks is known. The Badger Creek Tuff erupted at 34.3 Ma (Ar/Ar sanidine) during the formation of the Mount Aetna caldera in the southern portion of the batholith. Our Pb-206/U-238 age for the Badger Creek Tuff is 34.47 +/- A 0.05. The only analyzed plutonic rocks of similar age to the Badger Creek Tuff are an extra-caldera dike with a Pb-206/U-238 age of 34.57 +/- A 0.08 Ma, a ring dike with a Pb-206/U-238 age of 34.48 +/- A 0.09 Ma, and a portion of the Mount Aetna pluton with a Pb-206/U-238 age of 34.60 +/- A 0.13 Ma. The small volume intrusions related to the eruption of the Badger Creek Tuff are chemically similar to the ignimbrite and show no signature of crystal-liquid separation in the shallow crust. C1 [Mills, Ryan D.; Coleman, Drew S.] Univ N Carolina, Chapel Hill, NC 27599 USA. RP Mills, RD (reprint author), NASA, Astromat Res & Explorat Sci Directorate, JSC, Houston, TX 77058 USA. EM ryan.d.mills@nasa.gov FU National Science Foundation [EAR-1050215]; Geological Society of America; Sigma Xi; UNC Martin Fund FX Supported by National Science Foundation Grant EAR-1050215. Mills was also supported by the Geological Society of America, Sigma Xi, and the UNC Martin Fund. Laboratory assistance from Jesse Davis, Kyle Samperton, Jan Tympel, and Stephen Hughes was extremely helpful. Field work was completed with the help of Matt Zimmerer, Bill McIntosh, and Scott Bennett. We thank Jim Shannon and Peter Lipman for leading an informal field trip through the Mount Princeton area in 2007. Informal reviews by Mike Ackerson, Ryan Frazer, Allen Glazner, Peter Lipman, and Matt Zimmerer on earlier versions of this manuscript helped refine many of the concepts. Journal reviews by Calvin Miller, Shan de Silva, and editor Jon Blundy greatly improved the quality of the final publication. We also thank Jon Blundy for his editorial handling of the manuscript. NR 104 TC 16 Z9 16 U1 0 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0010-7999 J9 CONTRIB MINERAL PETR JI Contrib. Mineral. Petrol. PD MAY PY 2013 VL 165 IS 5 BP 961 EP 980 DI 10.1007/s00410-012-0843-4 PG 20 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 124MS UT WOS:000317469200007 ER PT J AU Ludovisi, D Cha, SS Ramachandran, NR Worek, WM AF Ludovisi, Daniele Cha, Soyoung S. Ramachandran, Narayanan R. Worek, William M. TI Systematic non-dimensional parametric investigation for the thermo-fluid dynamics of two-layered fluid systems (vol 56, pg 787, 2013) SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Correction C1 [Ludovisi, Daniele; Cha, Soyoung S.] Univ Illinois, Dept Mech & Ind Engn, Chicago, IL 60607 USA. [Ramachandran, Narayanan R.] NASA, George C Marshall Space Flight Ctr, Jacobs ESTS Grp, Huntsville, AL 35812 USA. [Worek, William M.] Michigan Technol Univ, Dept Mech Engn, Houghton, MI 49931 USA. RP Worek, WM (reprint author), Michigan Technol Univ, Dept Mech Engn, Houghton, MI 49931 USA. EM wworek@mtu.edu NR 1 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 0017-9310 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD MAY PY 2013 VL 60 BP 30 EP 30 DI 10.1016/j.ijheatmasstransfer.2012.11.062 PG 1 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 125IW UT WOS:000317534500005 ER PT J AU Nagaraja, MP Risin, D AF Nagaraja, Mamta Patel Risin, Diana TI The current state of bone loss research: Data from spaceflight and microgravity simulators SO JOURNAL OF CELLULAR BIOCHEMISTRY LA English DT Article DE BONE LOSS; SPACEFLIGHT; DISUSE; ASTRONAUTS; OSTEOPOROSIS ID BODY NEGATIVE-PRESSURE; RANDOM POSITIONING MACHINE; ROTATING WALL VESSEL; SPACE-FLIGHT; GENE-EXPRESSION; BED REST; MODELED MICROGRAVITY; 3-DIMENSIONAL CLINOSTAT; TREADMILL EXERCISE; 2T3 PREOSTEOBLASTS AB Bone loss is a well documented phenomenon occurring in humans both in short- and in long-term spaceflights. This phenomenon can be also reproduced on the ground in human and animals and also modeled in cell-based analogs. Since space flights are infrequent and expensive to study the biomedical effects of microgravity on the human body, much of the known pathology of bone loss comes from experimental studies. The most commonly used in vitro simulators of microgravity are clinostats while in vivo simulators include the bed rest studies in humans and hindlimb unloading experiments in animals. Despite the numerous reports that have documented bone loss in wide ranges in multiple crew members, the pathology remains a key concern and development of effective countermeasures is still a major task. Thus far, the offered modalities have not shown much success in preventing or alleviating bone loss in astronauts and cosmonauts. The objective of this review is to capture the most recent research on bone loss from spaceflights, bed rest and hindlimb unloading, and in vitro studies utilizing cellular models in clinostats. Additionally, this review offers projections on where the research has to focus to ensure the most rapid development of effective countermeasures. J. Cell. Biochem. 114: 10011008, 2013. (c) 2012 Wiley Periodicals, Inc. C1 [Nagaraja, Mamta Patel; Risin, Diana] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Nagaraja, MP (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM mamta.nagaraja@nasa.gov NR 62 TC 21 Z9 26 U1 4 U2 36 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0730-2312 J9 J CELL BIOCHEM JI J. Cell. Biochem. PD MAY PY 2013 VL 114 IS 5 BP 1001 EP 1008 DI 10.1002/jcb.24454 PG 8 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 108YL UT WOS:000316332200005 PM 23150462 ER PT J AU Stenger, MB Lee, SMC Westby, CM Ribeiro, LC Phillips, TR Martin, DS Platts, SH AF Stenger, Michael B. Lee, Stuart M. C. Westby, Christian M. Ribeiro, L. Christine Phillips, Tiffany R. Martin, David S. Platts, Steven H. TI Abdomen-High Elastic Gradient Compression Garments During Post-Spaceflight Stand Tests SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE anti-gravity suit; orthostatic intolerance; Space Shuttle ID ORTHOSTATIC INTOLERANCE; HYPOTENSION; ASTRONAUTS AB Space Shuttle astronauts wore an inflatable antigravity suit during re-entry and landing, and astronauts and cosmonauts wear an elastic-compression garment (with lacing) during Soyuz re-entry and landings and in the first few days of recovery. However, neither garment is an ideal countermeasure to spaceflight-induced orthostatic intolerance. Our laboratory has been investigating an elastic graded compression garment (GCG) that applies graduated pressures from the feet to the abdomen for use following International Space Station missions and possibly during exploration missions. Methods: Before and after Shuttle missions, 14 astronauts participated in a 3.5-min stand test. The stand test was conducted without garments preflight. On landing day, 7 astronauts wore the GCG while 7 astronauts did not (controls). Heart rate and blood pressure were measured in all astronauts during prone rest and standing. Stroke volume and cardiac output were measured only in GCG subjects. Results: No astronauts in either group became presyncopal during the stand test preflight or postflight. The change in heart rate from prone to standing was lower in the GCG subjects on landing day than in the control subjects. Within the GCG subjects only, the increase in total peripheral resistance from prone to standing was higher after spaceflight. Conclusions: The GCG prevented tachycardia and increased total peripheral resistance with standing after spaceflight. The GCG shows promise as a countermeasure against post-spaceflight orthostatic intolerance, can be easily donned, and is relatively comfortable to wear, but has not been validated after long-duration spaceflight. C1 [Stenger, Michael B.; Lee, Stuart M. C.; Ribeiro, L. Christine; Phillips, Tiffany R.; Martin, David S.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA. [Westby, Christian M.] Univ Space Res Assoc, Houston, TX USA. [Platts, Steven H.] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA. RP Stenger, MB (reprint author), Wyle Sci Technol & Engn Grp, 1290 Hercules Blvd,Suite 120, Houston, TX 77058 USA. EM michael.b.stenger@nasa.gov NR 20 TC 3 Z9 3 U1 1 U2 5 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD MAY PY 2013 VL 84 IS 5 BP 459 EP 466 DI 10.3357/ASEM.3528.2013 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AD1LR UT WOS:000332996000001 PM 23713210 ER PT J AU Tesch, PA Pozzo, M Ainegren, M Swaren, M Linnehan, RM AF Tesch, Per A. Pozzo, Marco Ainegren, Mats Swaren, Mikael Linnehan, Richard M. TI Cardiovascular Responses to Rowing on a Novel Ergometer Designed for Both Resistance and Aerobic Training in Space SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE aerobic power; astronaut health and fitness; cardiovascular deconditioning ID HUMAN SKELETAL-MUSCLE; BED REST; RESISTIVE EXERCISE; KNEE EXTENSOR; SIZE; SPACEFLIGHT; FLYWHEEL; STATION AB Background: Astronauts are required to perform both resistance and aerobic exercise while in orbit. This study assessed the aerobic energy yield and related physiological measurements using a nongravity dependent flywheel device designed for both resistance and aerobic exercise (RAD) in space. Methods: Eight physically active men and women performed all-out rowing on the RAD. For comparison, exercise was also carried out employing a commercially available rowing ergometer (C2). Results: Peak oxygen uptake during exercise using RAD and C2 averaged 3.11 +/- 0.49 and 3.18 +/- 0.50 L . min(-1), respectively. Similarly, peak plasma lactate concentration (9.6 vs. 11.2 mmol . L-1), heart rate (1 83 vs. 184 bpm), and rate of perceived exertion (15.8 vs. 16.0) were comparable across exercise using the two devices. Discussion: Collectively, the results suggest that this novel exercise modality offers cardiovascular and metabolic responses, and thus aerobic exercise stimulus that is equally effective as that evoked by established technology for indoor rowing. Given the need for physiologically sound and highly effective exercise countermeasures that features small mass and envelope, and allows for resistance and aerobic exercise in a single apparatus, we believe this novel hardware should be considered for use in space. C1 [Tesch, Per A.; Pozzo, Marco] Karolinska Inst, Dept Physiol & Pharmacol, Stockholm, Sweden. [Tesch, Per A.; Ainegren, Mats] Mid Sweden Univ, Dept Engn & Sustainable Dev, Ostersund, Sweden. [Swaren, Mikael] Mid Sweden Univ, Dept Hlth Sci, Ostersund, Sweden. [Linnehan, Richard M.] NASA, Lyndon B Johnson Space Ctr, Astronaut Off, Houston, TX 77058 USA. RP Tesch, PA (reprint author), Karolinska Inst, Dept Physiol & Pharmacol, Stockholm, Sweden. EM per.tesch@ki.se FU Swedish National Space Board (SNSB); European Union (EU; Mid Sweden University); European Space Agency (ESA) FX This study was supported by grants from the Swedish National Space Board (SNSB; PAT) and the European Union (EU; Mid Sweden University). Marco Pozzo was on a research fellowship sponsored by the European Space Agency (ESA). The technical assistance by Dr. Hans Berg, Mr. Anders Lund, Mr. Jesper Ostberg, and Ms. Monica Landin is greatly acknowledged. Authors of this paper have presented preliminary results related to this study at the 3rd European Congress on Achievements in Space Medicine into Health Care Practice and Industry, Berlin, Germany, September 29, 2005; the 9th Kongress Medizin und Mobilitat and 45th Jahrestagung Deutsche Gesellschaft fur Luft- und Raumfahrtmedizin e.v., Cologne, Germany, September 14,2007; the 13th Annual European College of Sport Science Meeting, Estoril, Portugal, July 11, 2008; the 33rd Annual Gravitational Physiology Meeting, Trieste, Italy, June 15, 2010; and the ELGRA Biennial Symposium, September 9, 2011, Antwerp, Belgium. NR 19 TC 6 Z9 6 U1 0 U2 4 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD MAY PY 2013 VL 84 IS 5 BP 516 EP 521 DI 10.3357/ASEM.3552.2013 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AD1LR UT WOS:000332996000009 PM 23713218 ER PT J AU Woike, MR Abdul-Aziz, A AF Woike, Mark R. Abdul-Aziz, Ali TI Health Monitoring and Crack Detection System Development for Turbine Engine Rotating Components SO MATERIALS EVALUATION LA English DT Article DE health monitoring; rotor; imbalance; spin test; crack detection; bode plot AB `The hot section components of jet engines undergo severe environmental operating conditions that generate combined thermo-mechanical loads, which impair their structural durability and performance. Minimizing the impact of these loads and inventing a crack detection technology to monitor the health of these components is among the key objectives of the National Aeronautics and Space Administration (NASA) Aviation Safety Program (AVSP). As a result, work is underway through the AVSP's Vehicle Systems Safety Technology (VSST) project to conduct research on ways to improve the safety and structural durability of engine hot section components, as well as to reduce cost and improve performance in every aircraft class. Therefore, it is NASA's goal to develop a robust health monitoring technique by means of in-situ and wireless detection technology and by expanding on sensor systems capable of functioning in severe environments, transmitting a signal upon detecting a predetermined crack length, and acting in an impartial fashion with respect to the overall performance of the engine system. Development and implementation of such sensor technology and diagnostic capabilities is possible only by conducting parallel analytical and experimental studies (coupon and subscale levels) to determine their applicability and success. Thus, ongoing research at NASA Glenn Research Center has aimed at investigating both global and local approaches for monitoring critical rotor components. This paper presents current ongoing research into health monitoring crack detection systems of turbine engine rotating components and their relevance on meeting the VSST program goals and milestones. Test data obtained under various operating conditions of a rotor disk with and without an artificially induced notch rotated at a rotational speed up to 12 000 rpm are presented, discussed and evaluated for health monitoring applications. Disk crack observations and related assessments from the collected data are reported. Lastly, analogous analytical results of disk spinning at a range of rotational speeds, showing the disk modal shapes and notch influence on damage initiation and crack propagation, are also included. C1 [Woike, Mark R.; Abdul-Aziz, Ali] NASA, Glenn Res Ctr, Opt Instrumentat & Nondestruct Evaluat Branch, Cleveland, OH 44135 USA. RP Woike, MR (reprint author), NASA, Glenn Res Ctr, Opt Instrumentat & Nondestruct Evaluat Branch, Cleveland, OH 44135 USA. NR 10 TC 0 Z9 0 U1 1 U2 2 PU AMER SOC NONDESTRUCTIVE TEST PI COLUMBUS PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA SN 0025-5327 J9 MATER EVAL JI Mater. Eval. PD MAY PY 2013 VL 71 IS 5 BP 571 EP 578 PG 8 WC Materials Science, Characterization & Testing SC Materials Science GA AR1GP UT WOS:000343334000006 ER PT J AU Peng, JZ Kim, E Piepmeier, J AF Peng, Jinzheng Kim, Edward Piepmeier, Jeffrey TI Global Simplified Atmospheric Radiative Transfer Model at L-Band SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Electromagnetic propagation; microwave radiometry; radiative transfer model (RTM) ID SALINITY AB A simplified atmospheric radiative transfer model at L-band has been developed for the Soil Moisture Active/Passive (SMAP) forward brightness temperature (level 1) simulator. The upwelling and downwelling brightness temperatures and the total loss factor of the atmosphere are modeled as polynomial functions of pressure, temperature, and water vapor density near the Earth's surface, as well as incidence angle. The model has been developed and verified by using global radiosonde data, and the model error is within the 0.1 K error budget (atmosphere portion) of the SMAP brightness temperature (Level 1B) product. C1 [Peng, Jinzheng] Morgan State Univ, Baltimore, MD 21251 USA. [Peng, Jinzheng; Kim, Edward; Piepmeier, Jeffrey] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Peng, JZ (reprint author), Morgan State Univ, Baltimore, MD 21251 USA. EM jzhpeng@umich.edu; ed.kim@nasa.gov; jeffrey.r.piepmeier@nasa.gov NR 7 TC 2 Z9 2 U1 0 U2 22 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD MAY PY 2013 VL 10 IS 3 BP 437 EP 440 DI 10.1109/LGRS.2012.2208213 PG 4 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 046YX UT WOS:000311802900005 ER PT J AU Le Vine, DM Abraham, S Utku, C Dinnat, EP AF Le Vine, David M. Abraham, Saji Utku, Cuneyt Dinnat, Emmanuel P. TI Aquarius Third Stokes Parameter Measurements: Initial Results SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Faraday rotation; microwave remote sensing; polarimetric radiometry ID SEA-SURFACE SALINITY; L-BAND; FARADAY-ROTATION; ANTENNA PATTERN; MISSION; SPACE; RADIOMETER; IONOSPHERE; WINDSAT; MODEL AB This letter reports a first look at the polarimetric (third Stokes parameter) channel on the Aquarius L-band radiometer that was launched in June of 2011 on the Aquarius/Satelite de Aplicaciones Cientificas (SAC)-D observatory. The primary purpose of the polarimetric channel is to provide an in situ measure of Faraday rotation which can be important for remote sensing at L-band, particularly in the case of sea surface salinity. However, it also provides an additional mode of observation and a chance to look for new features of the surface. Initial results show good agreement with expectations. In particular, the values of retrieved Faraday rotation agree with predicted values, and a nonzero signal is seen to occur over mixed scenes as predicted by theory. C1 [Le Vine, David M.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abraham, Saji] Wyle Informat Syst, Mclean, VA 22102 USA. [Utku, Cuneyt] NASA, Goddard Earth Sci Technol & Res, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dinnat, Emmanuel P.] Chapman Univ, Orange, CA 92866 USA. RP Le Vine, DM (reprint author), NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM saji.abraham-1@nasa.gov; cuneyt.utku@nasa.gov; emmanuel.dinnat@nasa.gov RI Dinnat, Emmanuel/D-7064-2012 OI Dinnat, Emmanuel/0000-0001-9003-1182 NR 17 TC 11 Z9 11 U1 0 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD MAY PY 2013 VL 10 IS 3 BP 520 EP 524 DI 10.1109/LGRS.2012.2211994 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 046YX UT WOS:000311802900022 ER PT J AU Gladkova, I Grossberg, M Bonev, G Romanov, P Riggs, G Hall, D AF Gladkova, Irina Grossberg, Michael Bonev, George Romanov, Peter Riggs, George Hall, Dorothy TI A Full Snow Season in Yellowstone: A Database of Restored Aqua Band 6 SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Aqua band 6; Moderate Resolution Imaging Spectroradiometer (MODIS); normalized difference snow index; restoration ID COVER PRODUCTS AB The algorithms for estimating snow extent for the Moderate Resolution Imaging Spectroradiometer (MODIS) optimally use the 1.6-mu m channel which is unavailable for MODIS on Aqua due to detector damage. As a test bed to demonstrate that Aqua band 6 can be restored, we chose the area surrounding Yellowstone and Grand Teton national parks. In such rugged and difficult-to-access terrain, satellite images are particularly important for providing an estimation of snow-cover extent. For the full 2010-2011 snow season covering the Yellowstone region, we have used quantitative image restoration to create a database of restored Aqua band 6. The database includes restored radiances, normalized vegetation index, normalized snow index, thermal data, and band-6-based snow-map products. The restored Aqua-band-6 data have also been regridded and combined with Terra data to produce a snow-cover map that utilizes both Terra and Aqua snow maps. Using this database, we show that the restored Aqua-band-6-based snow-cover extent has a comparable performance with respect to ground stations to the one based on Terra. The result of a restored band 6 from Aqua is that we have an additional band-6 image of the Yellowstone region each day. This image can be used to mitigate cloud occlusion, using the same algorithms used for band 6 on Terra. We show an application of this database of restored band-6 images to illustrate the value of creating a cloud gap filling using the National Aeronautics and Space Administration's operational cloud masks and data from both Aqua and Terra. C1 [Gladkova, Irina; Grossberg, Michael; Romanov, Peter] NOAA, Cooperat Remote Sensing Sci & Technol Ctr, New York, NY 10031 USA. [Bonev, George] CUNY, Grad Ctr, New York, NY 10016 USA. [Riggs, George; Hall, Dorothy] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gladkova, I (reprint author), NOAA, Cooperat Remote Sensing Sci & Technol Ctr, New York, NY 10031 USA. EM gladkova@cs.ccny.cuny.edu; grossberg@cs.ccny.cuny.edu; gbonev@gc.cuny.edu; Peter.Romanov@noaa.gov; george.a.riggs@nasa.gov; Dorothy.K.Hall@nasa.gov RI Romanov, Peter/F-5622-2010 OI Romanov, Peter/0000-0002-2153-8307 FU Center for Satellite Applications and Research, National Oceanic and Atmospheric Administration/National Environmental Satellite, Data, and Information Service [DG133E07CQ0077]; National Aeronautics and Space Administration's Earth Observing System Project FX This work was supported in part by Center for Satellite Applications and Research, National Oceanic and Atmospheric Administration/National Environmental Satellite, Data, and Information Service, under Grant DG133E07CQ0077. The works of D. Hall and G. Riggs were supported by the National Aeronautics and Space Administration's Earth Observing System Project. The views, opinions, and findings in this paper are those of the authors and should not be construed as an official NOAA and/or U.S. Government position, policy, or decision. NR 13 TC 0 Z9 0 U1 0 U2 27 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD MAY PY 2013 VL 10 IS 3 BP 553 EP 557 DI 10.1109/LGRS.2012.2213063 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 046YX UT WOS:000311802900029 ER PT J AU Aronica, GT Apel, H Di Baldassarre, G Schumann, GJP AF Aronica, Giuseppe T. Apel, Heiko Di Baldassarre, Giuliano Schumann, Guy J-P. TI HP - Special Issue on Flood Risk and Uncertainty Preface SO HYDROLOGICAL PROCESSES LA English DT Editorial Material C1 [Aronica, Giuseppe T.] Univ Messina, Dept Civil Engn, I-98143 Messina, Italy. [Apel, Heiko] GFZ German Res Ctr Geosci, Sect Hydrol 5 4, Potsdam, Germany. [Di Baldassarre, Giuliano] UNESCO IHE, Inst Water Educ, NL-2601 DA Delft, Netherlands. [Schumann, Guy J-P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Aronica, GT (reprint author), Univ Messina, Dept Civil Engn, I-98143 Messina, Italy. RI Di Baldassarre, Giuliano/C-7304-2009; Schumann, Guy/F-9760-2011; Apel, Heiko/G-6280-2013; OI Di Baldassarre, Giuliano/0000-0002-8180-4996; Apel, Heiko/0000-0002-8852-652X; Aronica, Giuseppe Tito/0000-0003-0485-6466 NR 0 TC 1 Z9 1 U1 1 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1099-1085 J9 HYDROL PROCESS JI Hydrol. Process. PD APR 30 PY 2013 VL 27 IS 9 SI SI BP 1291 EP 1291 DI 10.1002/hyp.9812 PG 1 WC Water Resources SC Water Resources GA 127DC UT WOS:000317674900002 ER PT J AU Wagner, JR Balaraman, GS Niesen, MJM Larsen, AB Jain, A Vaidehi, N AF Wagner, Jeffrey R. Balaraman, Gouthaman S. Niesen, Michiel J. M. Larsen, Adrien B. Jain, Abhinandan Vaidehi, Nagarajan TI Advanced techniques for constrained internal coordinate molecular dynamics SO JOURNAL OF COMPUTATIONAL CHEMISTRY LA English DT Article DE constrained dynamics; torsional dynamics; ab-initio folding; molecular dynamics; integration techniques; GNEIMO ID CLASSICAL STATISTICAL-MECHANICS; MASS OPERATOR METHOD; MULTIBODY SYSTEMS; SIMULATIONS; ALGORITHM; MOTION; EQUIPARTITION; EQUATIONS; POLYMERS AB Internal coordinate molecular dynamics (ICMD) methods provide a more natural description of a protein by using bond, angle, and torsional coordinates instead of a Cartesian coordinate representation. Freezing high-frequency bonds and angles in the ICMD model gives rise to constrained ICMD (CICMD) models. There are several theoretical aspects that need to be developed to make the CICMD method robust and widely usable. In this article, we have designed a new framework for (1) initializing velocities for nonindependent CICMD coordinates, (2) efficient computation of center of mass velocity during CICMD simulations, (3) using advanced integrators such as RungeKutta, Lobatto, and adaptive CVODE for CICMD simulations, and (4) cancelling out the flying ice cube effect that sometimes arises in NoseHoover dynamics. The Generalized NewtonEuler Inverse Mass Operator (GNEIMO) method is an implementation of a CICMD method that we have developed to study protein dynamics. GNEIMO allows for a hierarchy of coarse-grained simulation models based on the ability to rigidly constrain any group of atoms. In this article, we perform tests on the Lobatto and RungeKutta integrators to determine optimal simulation parameters. We also implement an adaptive coarse-graining tool using the GNEIMO Python interface. This tool enables the secondary structure-guided freezing and thawing of degrees of freedom in the molecule on the fly during molecular dynamics simulations and is shown to fold four proteins to their native topologies. With these advancements, we envision the use of the GNEIMO method in protein structure prediction, structure refinement, and in studying domain motion. (c) 2013 Wiley Periodicals, Inc. C1 [Wagner, Jeffrey R.; Balaraman, Gouthaman S.; Niesen, Michiel J. M.; Larsen, Adrien B.; Vaidehi, Nagarajan] City Hope Natl Med Ctr, Div Immunol, Beckman Res Inst, Duarte, CA 91010 USA. [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wagner, JR (reprint author), City Hope Natl Med Ctr, Div Immunol, Beckman Res Inst, Duarte, CA 91010 USA. EM nvaidehi@coh.org RI Niesen, Michiel/L-8985-2013 FU National Institute of Health [RO1GM082896]; NIH [RO1GM082896] FX Contract/grant sponsor: National Institute of Health; Contract/grant number: RO1GM082896; Contract/grant sponsor: NIH RO1GM082896 is the only grant that funded this project and not the SimBios grant. NR 40 TC 10 Z9 10 U1 0 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0192-8651 J9 J COMPUT CHEM JI J. Comput. Chem. PD APR 30 PY 2013 VL 34 IS 11 BP 904 EP 914 DI 10.1002/jcc.23200 PG 11 WC Chemistry, Multidisciplinary SC Chemistry GA 112XG UT WOS:000316627400002 PM 23345138 ER PT J AU Kim, W Tengra, FK Young, Z Shong, J Marchand, N Chan, HK Pangule, RC Parra, M Dordick, JS Plawsky, JL Collins, CH AF Kim, Wooseong Tengra, Farah K. Young, Zachary Shong, Jasmine Marchand, Nicholas Chan, Hon Kit Pangule, Ravindra C. Parra, Macarena Dordick, Jonathan S. Plawsky, Joel L. Collins, Cynthia H. TI Spaceflight Promotes Biofilm Formation by Pseudomonas aeruginosa SO PLOS ONE LA English DT Article ID SHEAR MODELED MICROGRAVITY; MULTICELLULAR STRUCTURES; ESCHERICHIA-COLI; GENE-EXPRESSION; IV PILI; MOTILITY; GROWTH; VIRULENCE; FLAGELLAR; SYSTEM AB Understanding the effects of spaceflight on microbial communities is crucial for the success of long-term, manned space missions. Surface-associated bacterial communities, known as biofilms, were abundant on the Mir space station and continue to be a challenge on the International Space Station. The health and safety hazards linked to the development of biofilms are of particular concern due to the suppression of immune function observed during spaceflight. While planktonic cultures of microbes have indicated that spaceflight can lead to increases in growth and virulence, the effects of spaceflight on biofilm development and physiology remain unclear. To address this issue, Pseudomonas aeruginosa was cultured during two Space Shuttle Atlantis missions: STS-132 and STS-135, and the biofilms formed during spaceflight were characterized. Spaceflight was observed to increase the number of viable cells, biofilm biomass, and thickness relative to normal gravity controls. Moreover, the biofilms formed during spaceflight exhibited a column-and-canopy structure that has not been observed on Earth. The increase in the amount of biofilms and the formation of the novel architecture during spaceflight were observed to be independent of carbon source and phosphate concentrations in the media. However, flagella-driven motility was shown to be essential for the formation of this biofilm architecture during spaceflight. These findings represent the first evidence that spaceflight affects community-level behaviors of bacteria and highlight the importance of understanding how both harmful and beneficial human-microbe interactions may be altered during spaceflight. C1 [Kim, Wooseong; Tengra, Farah K.; Young, Zachary; Shong, Jasmine; Marchand, Nicholas; Chan, Hon Kit; Pangule, Ravindra C.; Dordick, Jonathan S.; Plawsky, Joel L.; Collins, Cynthia H.] Rensselaer Polytech Inst, Dept Chem & Biol Engn, Troy, NY 12180 USA. [Kim, Wooseong; Tengra, Farah K.; Shong, Jasmine; Marchand, Nicholas; Pangule, Ravindra C.; Dordick, Jonathan S.; Collins, Cynthia H.] Rensselaer Polytech Inst, Ctr Biotechnol & Interdisciplinary Studies, Troy, NY USA. [Parra, Macarena] Lockheed Martin, Ames Res Ctr, Moffett Field, CA USA. RP Collins, CH (reprint author), Rensselaer Polytech Inst, Dept Chem & Biol Engn, Troy, NY 12180 USA. EM ccollins@rpi.edu RI Kim, Wooseong/A-9256-2017 OI Kim, Wooseong/0000-0002-4597-8374 FU NASA [NNX09AI70G] FX This work was supported by NASA Grant NNX09AI70G to CHC. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 34 TC 26 Z9 27 U1 5 U2 60 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 29 PY 2013 VL 8 IS 4 AR e62437 DI 10.1371/journal.pone.0062437 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 181JC UT WOS:000321662800045 PM 23658630 ER PT J AU Jin, B Kang, D Kim, J Meyyappan, M Lee, JS AF Jin, Bo Kang, Daegun Kim, Jungsik Meyyappan, M. Lee, Jeong-Soo TI Thermally efficient and highly scalable In2Se3 nanowire phase change memory SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID MELTING TEMPERATURE; CELL; CONDUCTIVITY; TECHNOLOGY; DEVICES; FILMS; GE AB The electrical characteristics of nonvolatile In2Se3 nanowire phase change memory are reported. Size-dependent memory switching behavior was observed in nanowires of varying diameters and the reduction in set/reset threshold voltage was as low as 3.45 V/6.25V for a 60 nm nanowire, which is promising for highly scalable nanowire memory applications. Also, size-dependent thermal resistance of In2Se3 nanowire memory cells was estimated with values as high as 5.86 x 10(13) and 1.04 x 10(6) K/W for a 60 nm nanowire memory cell in amorphous and crystalline phases, respectively. Such high thermal resistances are beneficial for improvement of thermal efficiency and thus reduction in programming power consumption based on Fourier's law. The evaluation of thermal resistance provides an avenue to develop thermally efficient memory cell architecture. (C) 2013 AIP Publishing LLC C1 [Jin, Bo; Kim, Jungsik; Meyyappan, M.; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea. [Kang, Daegun] Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang 790784, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Meyyappan, M (reprint author), Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea. EM m.meyyappan@nasa.gov; ljs6951@postech.ac.kr FU World Class University; Ministry of Education, Science and Technology through the National Research Foundation of Korea [R31-10100]; Center for Advanced Soft Electronics under the Global Frontier Research Program of the Ministry of Education, Science and Technology, Korea [2011-0031638]; Pohang University of Science and Technology; Samsung Electronics Co., Ltd. FX This research was supported by World Class University program funded by the Ministry of Education, Science and Technology through the National Research Foundation of Korea (R31-10100); by a grant (Code No. 2011-0031638) from the Center for Advanced Soft Electronics under the Global Frontier Research Program of the Ministry of Education, Science and Technology, Korea; by Semiconductor Industry Collaborative Project between Pohang University of Science and Technology and Samsung Electronics Co., Ltd. NR 40 TC 8 Z9 8 U1 1 U2 38 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD APR 28 PY 2013 VL 113 IS 16 AR 164303 DI 10.1063/1.4802672 PG 6 WC Physics, Applied SC Physics GA 138ZF UT WOS:000318550300053 ER EF