FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Schott, J Gerace, A Brown, S Gartley, M Montanaro, M Reuter, DC AF Schott, John Gerace, Aaron Brown, Scott Gartley, Michael Montanaro, Matthew Reuter, Dennis C. TI Simulation of Image Performance Characteristics of the Landsat Data Continuity Mission (LDCM) Thermal Infrared Sensor (TIRS) SO REMOTE SENSING LA English DT Article DE Landsat; TIRS; thermal; DIRSIG; simulated imagery; image quality ID ON-ORBIT AB The next Landsat satellite, which is scheduled for launch in early 2013, will carry two instruments: the Operational Land Imager (OLI) and the Thermal Infrared Sensor (TIRS). Significant design changes over previous Landsat instruments have been made to these sensors to potentially enhance the quality of Landsat image data. TIRS, which is the focus of this study, is a dual-band instrument that uses a push-broom style architecture to collect data. To help understand the impact of design trades during instrument build, an effort was initiated to model TIRS imagery. The Digital Imaging and Remote Sensing Image Generation (DIRSIG) tool was used to produce synthetic "on-orbit" TIRS data with detailed radiometric, geometric, and digital image characteristics. This work presents several studies that used DIRSIG simulated TIRS data to test the impact of engineering performance data on image quality in an effort to determine if the image data meet specifications or, in the event that they do not, to determine if the resulting image data are still acceptable. C1 [Schott, John; Gerace, Aaron; Brown, Scott; Gartley, Michael] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Montanaro, Matthew] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. RP Schott, J (reprint author), Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM schott@cis.rit.edu; gerace@cis.rit.edu; brown@cis.rit.edu; gartley@cis.rit.edu; matthew.montanaro@nasa.gov; Dennis.C.Reuter@mail.nasa.gov NR 17 TC 9 Z9 9 U1 0 U2 19 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD AUG PY 2012 VL 4 IS 8 BP 2477 EP 2491 DI 10.3390/rs4082477 PG 15 WC Remote Sensing SC Remote Sensing GA 003CW UT WOS:000308586800016 ER PT J AU Harris, AI Sieth, M Lau, JM Church, SE Samoska, LA Cleary, K AF Harris, A. I. Sieth, M. Lau, J. M. Church, S. E. Samoska, L. A. Cleary, K. TI Note: Cryogenic microstripline-on-Kapton microwave interconnects SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article AB Simple broadband microwave interconnects are needed for increasing the size of focal plane heterodyne radiometer arrays. We have measured loss and crosstalk for arrays of microstrip transmission lines in flex circuit technology at 297 and 77 K, finding good performance to at least 20 GHz. The dielectric constant of Kapton substrates changes very little from 297 to 77 K, and the electrical loss drops. The small cross-sectional area of metal in a printed circuit structure yields overall thermal conductivities similar to stainless steel coaxial cable. Operationally, the main performance tradeoffs are between crosstalk and thermal conductivity. We tested a patterned ground plane to reduce heat flux. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4737185] C1 [Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Sieth, M.; Lau, J. M.; Church, S. E.] Stanford Univ, Dept Phys, Palo Alto, CA 94305 USA. [Samoska, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cleary, K.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Harris, AI (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM harris@astro.umd.edu FU NSF [ATI-0905855] FX This work was supported by NSF Grant No. ATI-0905855 (ARRA). We thank A. W. R. for providing access to Microwave Office under its University Program. We benefited from conversations with Dr. M. Morgan of the National Radio Astronomy Observatory. NR 6 TC 7 Z9 7 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD AUG PY 2012 VL 83 IS 8 AR 086105 DI 10.1063/1.4737185 PG 3 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 000RU UT WOS:000308406500081 PM 22938347 ER PT J AU Ramanathan, A Muniz, SR Wright, KC Anderson, RP Phillips, WD Helmerson, K Campbell, GK AF Ramanathan, Anand Muniz, Sergio R. Wright, Kevin C. Anderson, Russell P. Phillips, William D. Helmerson, Kristian Campbell, Gretchen K. TI Partial-transfer absorption imaging: A versatile technique for optimal imaging of ultracold gases SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID BOSE-EINSTEIN CONDENSATION; ATOMS; PHYSICS; SYSTEM AB Partial-transfer absorption imaging is a tool that enables optimal imaging of atomic clouds for a wide range of optical depths. In contrast to standard absorption imaging, the technique can be minimally destructive and can be used to obtain multiple successive images of the same sample. The technique involves transferring a small fraction of the sample from an initial internal atomic state to an auxiliary state and subsequently imaging that fraction absorptively on a cycling transition. The atoms remaining in the initial state are essentially unaffected. We demonstrate the technique, discuss its applicability, and compare its performance as a minimally destructive technique to that of phase-contrast imaging. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4747163] C1 Natl Inst Stand & Technol, Joint Quantum Inst, Gaithersburg, MD 20899 USA. Univ Maryland, Gaithersburg, MD 20899 USA. RP Ramanathan, A (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Mail Code 694, Greenbelt, MD 20771 USA. EM gretchen.campbell@nist.gov RI Anderson, Russell/H-1167-2011; Campbell, Gretchen/E-8338-2010; Muniz, Sergio/G-6426-2012; Helmerson, Kristian/E-3683-2013; Wright, Kevin/N-3207-2013; OI Anderson, Russell/0000-0002-4495-7926; Campbell, Gretchen/0000-0003-2596-1919; Muniz, Sergio/0000-0002-8753-4659; Wright, Kevin/0000-0001-6202-1737; Ramanathan, Anand/0000-0002-1865-0904 FU ONR; ARO atomtronics MURI; NSF PFC at JQI FX We would like to thank S. L. Rolston and W. T. Hill for helpful discussions, and R. B. Blakestad for a careful reading of the manuscript. This work was partially supported by ONR, the ARO atomtronics MURI, and the NSF PFC at JQI. NR 31 TC 17 Z9 17 U1 4 U2 16 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD AUG PY 2012 VL 83 IS 8 AR 083119 DI 10.1063/1.4747163 PG 9 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 000RU UT WOS:000308406500020 PM 22938286 ER PT J AU Scott, VJ Tse, M Shearn, MJ Siegel, PH Amashukeli, X AF Scott, Valerie J. Tse, Margaret Shearn, Michael J. Siegel, Peter H. Amashukeli, Xenia TI An RF-powered micro-reactor for the detection of astrobiological target molecules on planetary bodies SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID OMEGA/MARS EXPRESS; MARS; WATER; CHEMISTRY; MERIDIANI; EVOLUTION; SURFACE; SOIL AB We describe a sample-processing micro-reactor that utilizes 60 GHz RF radiation with approximately 730 mW of output power. The instrument design and performance characterization are described and then illustrated with modeling and experimental studies. The micro-reactor's efficiency on affecting hydrolysis of chemical bonds similar to those within large complex molecules was demonstrated: a disaccharide-sucrose-was hydrolyzed completely under micro-reactor conditions. The products of the micro-reactor-facilitated hydrolysis were analyzed using mass spectroscopy and proton nuclear magnetic resonance analytical techniques. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4746994] C1 [Scott, Valerie J.; Tse, Margaret; Shearn, Michael J.; Siegel, Peter H.; Amashukeli, Xenia] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Amashukeli, X (reprint author), CALTECH, 1200 E Calif Blvd,MC 132-80, Pasadena, CA 91125 USA. EM Xenia.Amashukeli@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA); NASA FX The research described in this paper was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration. The research was supported through the National Aeronautics and Space Administration (NASA) Planetary Instrument Definition and Development Program; Dr. V. Scott received support through the NASA Postdoctoral Program. NR 28 TC 2 Z9 2 U1 0 U2 4 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 AUG PY 2012 VL 83 IS 8 AR 084102 DI 10.1063/1.4746994 PG 7 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 000RU UT WOS:000308406500047 PM 22938313 ER PT J AU Jain, A Park, IH Vaidehi, N AF Jain, Abhinandan Park, In-Hee Vaidehi, Nagarajan TI Equipartition Principle for Internal Coordinate Molecular Dynamics SO JOURNAL OF CHEMICAL THEORY AND COMPUTATION LA English DT Article ID CLASSICAL STATISTICAL-MECHANICS; CONSTRAINED DYNAMICS; GENERAL-THEORY; POLYMER-CHAIN; SIMULATION; PARTITION AB The principle of equipartition of (kinetic) energy for all atom Cartesian molecular dynamics states that each momentum phase space coordinate on the average has kT/2 of kinetic energy in a canonical ensemble. This principle is used in molecular dynamics simulations to initialize velocities, and to calculate statistical properties such as entropy. Internal coordinate molecular dynamics (ICMD) models differ from Cartesian models in that the overall kinetic energy depends on the generalized coordinates and includes cross-terms Due to this coupled structure, no such equipartition principle holds for ICMD models. In this paper, we introduce noncanonical modal coordinates to recover some of the structural simplicity of Cartesian models and develop a new equipartition principle for ICMD models. We derive low order recursive computational algorithms for transforming between the modal and physical coordinates. The equipartition principle in modal coordinates provides a rigorous method for initializing velocities in ICMD simulations, thus replacing the ad hoc methods used until now It also sets the basis for calculating conformational entropy using internal coordinates. C1 [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Park, In-Hee; Vaidehi, Nagarajan] Beckman Res Inst City Hope, Div Immunol, Duarte, CA 91010 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Abhi.Jain@jpl.nasa.gov; nvaidehi@coh.org RI Park, In-Hee/D-5364-2013 FU National Aeronautics and Space Administration; National Institute of Health [RO1GM082896-01A2] FX The research described in this paper was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration, in collaboration with Beckman Research Institute of the City of Hope. This project was also supported in part by Grant Number RO1GM082896-01A2 from the National Institute of Health. NR 28 TC 12 Z9 12 U1 0 U2 7 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1549-9618 J9 J CHEM THEORY COMPUT JI J. Chem. Theory Comput. PD AUG PY 2012 VL 8 IS 8 BP 2581 EP 2587 DI 10.1021/ct3002046 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 988GZ UT WOS:000307478800005 PM 23341754 ER PT J AU Roberge, A Chen, CH Millan-Gabet, R Weinberger, AJ Hinz, PM Stapelfeldt, KR Absil, O Kuchner, MJ Bryden, G AF Roberge, Aki Chen, Christine H. Millan-Gabet, Rafael Weinberger, Alycia J. Hinz, Philip M. Stapelfeldt, Karl R. Absil, Olivier Kuchner, Marc J. Bryden, Geoffrey TI The Exozodiacal Dust Problem for Direct Observations of Exo-Earths SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SOLAR-TYPE STARS; DISCOVERED DEBRIS DISKS; BETA-PICTORIS; RESONANT SIGNATURES; EPSILON-ERIDANI; SPACE; RING; ANALOGS; SYSTEM; AU AB Debris dust in the habitable zones of stars-otherwise known as exozodiacal dust-comes from extrasolar asteroids and comets and is thus an expected part of a planetary system. Background flux from the solar system's zodiacal dust and the exozodiacal dust in the target system is likely to be the largest source of astrophysical noise in direct observations of terrestrial planets in the habitable zones of nearby stars. Furthermore, dust structures like clumps, thought to be produced by dynamical interactions with exoplanets, are a possible source of confusion. In this article, we qualitatively assess the primary impact of exozodiacal dust on high-contrast direct imaging at optical wavelengths, such as would be performed with a coronagraph. Then we present the sensitivity of previous, current, and near-term facilities to thermal emission from debris dust at all distances from nearby solar-type stars, as well as our current knowledge of dust levels from recent surveys. Finally, we address the other method of detecting debris dust, through high-contrast imaging in scattered light. This method is currently far less sensitive than thermal emission observations, but provides high spatial resolution for studying dust structures. This article represents the first report of NASA's Exoplanet Exploration Program Analysis Group (ExoPAG). C1 [Roberge, Aki; Stapelfeldt, Karl R.; Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Chen, Christine H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Millan-Gabet, Rafael] NASA, CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Hinz, Philip M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Absil, Olivier] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium. [Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Roberge, A (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. EM Aki.Roberge@nasa.gov; cchen@stsci.edu; rafael@ipac.caltech.edu; alycia@dtm.ciw.edu; phinz@as.arizona.edu; Karl.R.Stapelfeldt@nasa.gov; absil@astro.ulg.ac.be; Marc.Kuchner@nasa.gov; Geoff.Bryden@jpl.nasa.gov RI Roberge, Aki/D-2782-2012; OI Roberge, Aki/0000-0002-2989-3725; Weinberger, Alycia/0000-0001-6654-7859; Absil, Olivier/0000-0002-4006-6237 NR 47 TC 23 Z9 23 U1 2 U2 5 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 AUG PY 2012 VL 124 IS 918 BP 799 EP 808 DI 10.1086/667218 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007UQ UT WOS:000308914300001 ER PT J AU Fernlund, E Liuba, P Platonov, P Carlson, J Schlegel, TT AF Fernlund, E. Liuba, P. Platonov, P. Carlson, J. Schlegel, T. T. TI MYBPC3 hypertrophic cardiomyopathy can be detected by using advanced ECG in children and young adults SO EUROPEAN HEART JOURNAL LA English DT Meeting Abstract CT Congress of the European-Society-of-Cardiology (ESC) CY AUG 25-29, 2012 CL Munchen, GERMANY SP European Soc Cardiol (ESC) C1 [Fernlund, E.; Liuba, P.] Lund Univ, Skane Univ Hosp, Childrens Heart Ctr, Lund, Sweden. [Platonov, P.; Carlson, J.] Lund Univ, Skane Univ Hosp, Dept Cardiol, Lund, Sweden. [Schlegel, T. T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0195-668X J9 EUR HEART J JI Eur. Heart J. PD AUG PY 2012 VL 33 SU 1 BP 575 EP 575 PG 1 WC Cardiac & Cardiovascular Systems SC Cardiovascular System & Cardiology GA 995MO UT WOS:000308012404337 ER PT J AU Gibson, CR Mader, TH Schallhorn, SC Pesudovs, K Lipsky, W Raid, E Jennings, RT Fogarty, JA Garriott, RA Garriott, OK Johnston, SL AF Gibson, C. Robert Mader, Thomas H. Schallhorn, Steven C. Pesudovs, Konrad Lipsky, William Raid, Elias Jennings, Richard T. Fogarty, Jennifer A. Garriott, Richard A. Garriott, Owen K. Johnston, Smith L. TI Visual stability of laser vision correction in an astronaut on a Soyuz mission to the International Space Station SO JOURNAL OF CATARACT AND REFRACTIVE SURGERY LA English DT Article ID FRONT-GUIDED LASIK; PHOTOREFRACTIVE KERATECTOMY; EXCIMER-LASER; INTRAOCULAR-PRESSURE; CORNEAL TOPOGRAPHY; LIGHT-FLASHES; FOLLOW-UP; MYOPIA; SURGERY; PERFORMANCE AB This report documents the effects of photorefractive keratectomy (PRK) in an astronaut during a 12-day Russian Soyuz mission to the International Space Station in 2008. Changing environmental conditions of launch, microgravity exposure, and reentry create an extremely dynamic ocular environment. Although many normal eyes have repeatedly been subject to such stresses, the effect on an eye with a relatively thin cornea as a result of PRK has not been reported. This report suggests that PRK is a safe, effective, and well-tolerated procedure in astronauts during space flight. Financial Disclosure: No author has a financial or proprietary interest in any material or method mentioned. J Cataract Refract Surg 2012; 38:1486-1491 (C) 2012 ASCRS and ESCRS C1 [Gibson, C. Robert; Lipsky, William] Johnson Space Ctr, Coastal Eye Associates, Webster & Wyle Integrated Sci & Engn, Houston, TX USA. [Fogarty, Jennifer A.; Johnston, Smith L.] Johnson Space Ctr, Space Med Div, Natl Aeronaut & Space Adm, Houston, TX USA. [Jennings, Richard T.] Univ Texas Med Branch, Galveston, TX USA. [Mader, Thomas H.] Alaska Native Med Ctr, Dept Ophthalmol, Anchorage, AK USA. [Schallhorn, Steven C.] Univ Calif San Francisco, San Francisco, CA 94143 USA. [Schallhorn, Steven C.] Opt Express, San Diego, CA USA. [Garriott, Richard A.] Space Adventures, Vienna, VA USA. [Pesudovs, Konrad] Flinders Med Ctr, NH&MRC Ctr Clin Eye Res, Dept Optometry & Vis Sci, Bedford Pk, SA, Australia. Flinders Univ S Australia, Bedford Pk, SA, Australia. [Raid, Elias] European Med Ctr, Moscow, Russia. [Garriott, Owen K.] NASA, Washington, DC USA. RP Gibson, CR (reprint author), Coastal Eye Associates, Webster & Wyle Integrated Sci & Engn, 555 E Med Ctr Blvd, Webster, TX 77598 USA. EM charles.gibson-1@nasa.gov RI Johnston, Sebastian/I-2423-2012; OI Pesudovs, Konrad/0000-0002-6322-9369 NR 43 TC 4 Z9 4 U1 0 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0886-3350 J9 J CATARACT REFR SURG JI J. Cataract. Refract. Surg. PD AUG PY 2012 VL 38 IS 8 BP 1486 EP 1491 DI 10.1016/j.jcrs.2012.06.012 PG 6 WC Ophthalmology; Surgery SC Ophthalmology; Surgery GA 986EB UT WOS:000307322700027 PM 22814056 ER PT J AU Zaman, KBMQ AF Zaman, K. B. M. Q. TI Effect of Initial Boundary-Layer State on Subsonic Jet Noise SO AIAA JOURNAL LA English DT Article ID SHEAR-LAYER AB Significant differences in subsonic jet noise databases have been reported in recent review papers. Specifically, university-type facilities involving higher contraction ratios and possibly cleaner flows are noted to yield higher levels or noise relative to data from industrial-type facilities. An experimental investigation is carried out in an attempt to understand the sources of the anomaly. It is inferred that differences in jet core turbulence may not be the source. An observation in a previous study is confirmed showing that two nozzles of the same diameter but different internal geometry can produce a difference in subsonic jet noise. The present measurements demonstrate that the noisier nozzle involves a highly disturbed laminar, or nominally laminar, boundary-layer state as opposed to a turbulent state with the other. The former boundary-layer state with the noisier nozzle is actually marked by larger turbulence intensities, consistent with the higher radiated noise. Although the boundary-layer characteristics were not reported with the earlier databases, the present results suggest that differences therein might be a source of the anomaly. C1 NASA, John H Glenn Res Ctr Lewis Field, Inlet & Nozzle Branch, Aeroprop Div, Cleveland, OH 44135 USA. RP Zaman, KBMQ (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Inlet & Nozzle Branch, Aeroprop Div, Cleveland, OH 44135 USA. FU Supersonic Project under the Fundamental Aeronautics Program FX Support from the Supersonic Project under the Fundamental Aeronautics Program is gratefully acknowledged. NR 23 TC 11 Z9 11 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD AUG PY 2012 VL 50 IS 8 BP 1784 EP 1795 DI 10.2514/1.J051712 PG 12 WC Engineering, Aerospace SC Engineering GA 986FA UT WOS:000307325400012 ER PT J AU Bolmont, E Raymond, SN Leconte, J Matt, SP AF Bolmont, E. Raymond, S. N. Leconte, J. Matt, S. P. TI Effect of the stellar spin history on the tidal evolution of close-in planets SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: rotation; planets and satellites: dynamical evolution and stability; planet-star interactions ID LOW-MASS STARS; ANGULAR-MOMENTUM EVOLUTION; FULLY CONVECTIVE STARS; ORION NEBULA CLUSTER; SHORT-PERIOD PLANETS; ROTATIONAL EVOLUTION; LITHIUM DEPLETION; HOT JUPITER; TRANSIT SURVEY; GIANT PLANETS AB Context. The spin rate of stars evolves substantially during their lifetime, owing to the evolution of their internal structure and to external torques arising from the interaction of stars with their environments and stellar winds. Aims. We investigate how the evolution of the stellar spin rate affects, and is affected by, planets in close orbits via star-planet tidal interactions. Methods. We used a standard equilibrium tidal model to compute the orbital evolution of single planets orbiting both Sun-like stars and very low-mass stars (0.1 M-circle dot). We tested two stellar spin evolution profiles, one with fast initial rotation (1.2 day rotation period) and one with slow initial rotation (8 day period). We tested the effect of varying the stellar and planetary dissipations, and the planet's mass and initial orbital radius. Results. For Sun-like stars, the different tidal evolution between initially rapidly and slowly rotating stars is only evident for extremely close-in gas giants orbiting highly dissipative stars. However, for very low-mass stars the effect of the initial rotation of the star on the planet's evolution is apparent for less massive (1 M-circle dot) planets and typical dissipation values. We also find that planetary evolution can have significant effects on the stellar spin history. In particular, when a planet falls onto the star, it can cause the star to spin up. Conclusions. Tidal evolution allows us to differentiate between the early behaviors of extremely close-in planets orbiting either a rapidly rotating star or a slowly rotating star. The early spin-up of the star allows the close-in planets around fast rotators to survive the early evolution. For planets around M-dwarfs, surviving the early evolution means surviving on Gyr timescales, whereas for Sun-like stars the spin-down brings about late mergers of Jupiter planets. In the light of this study, we can say that differentiating one type of spin evolution from another given the present position of planets can be very tricky. Unless we can observe some markers of former evolution, it is nearly impossible to distinguish the two very different spin profiles, let alone intermediate spin-profiles. Nevertheless, some conclusions can still be drawn about statistical distributions of planets around fully convective M-dwarfs. If tidal evolution brings about a merger late in the stellar history, it can also entail a noticeable acceleration of the star at late ages, so that it is possible to have old stars that spin rapidly. This raises the question of how the age of stars can be more tightly constrained. C1 [Bolmont, E.; Raymond, S. N.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Bolmont, E.; Raymond, S. N.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Leconte, J.] Inst Pierre Simon Laplace, Lab Meteorol Dynam, F-75005 Paris, France. [Matt, S. P.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA, CNRS,INSU,Irfu, F-91191 Gif Sur Yvette, France. [Matt, S. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Bolmont, E (reprint author), Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. EM emeline.bolmont@obs.u-bordeaux1.fr OI Matt, Sean/0000-0001-9590-2274 FU CNRS's PNP program; ERC [207430 STARS2] FX We are grateful to Andrew West for suggesting that we study low-mass stars rather than simply concentrating on the case of Sun-like stars. We thank Franck Selsis and Franck Hersant for their ideas and support. We also thank the CNRS's PNP program for funding, and the Conseil Regional d'Aquitaine for help in purchasing the computers on which these calculations were performed. SPM acknowledges support by the ERC through grant 207430 STARS2 (http://www.stars2.eu). NR 71 TC 24 Z9 24 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2012 VL 544 AR A124 DI 10.1051/0004-6361/201219645 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100124 ER PT J AU Chamballu, A Bartlett, JG Melin, JB AF Chamballu, A. Bartlett, J. G. Melin, J. -B. TI The Planck SZ Cluster Catalog: expected X-ray properties SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general; X-rays: galaxies: clusters; galaxies: clusters: intracluster medium ID NEARBY GALAXY CLUSTERS; SOUTH-POLE TELESCOPE; MASS-TEMPERATURE RELATION; DARK-MATTER HALOES; REPRESENTATIVE SAMPLE; LUMINOSITY FUNCTION; INTRACLUSTER MEDIUM; SCALING RELATIONS; CHANDRA SAMPLE; POWER-SPECTRUM AB Surveys based on the Sunyaev-Zel'dovich (SZ) effect provide a fresh view of the galaxy cluster population, one that is complementary to X-ray surveys. To better understand the relation between these two kinds of survey, we construct an empirical cluster model using scaling relations constrained by current X-ray and SZ data. We apply our model to predict the X-ray properties of the Planck SZ Cluster Catalog (PCC) and compare them to existing X-ray cluster catalogs. We find that Planck should significantly extend the depth of the previous all-sky cluster survey, performed in the early 1990s by the ROSAT satellite, and should be particularly effective at finding hot, massive clusters (T > 6 keV) out to redshift unity. These are rare objects, and our findings suggest that Planck could increase the observational sample at z > 0.6 by an order of magnitude. This would open the way for detailed studies of massive clusters out to these higher redshifts. Specifically, we find that the majority of newly-detected Planck clusters should have X-ray fluxes 10(-13) erg/s/cm(2) < fX[0.5-2 keV] < 10-(12) erg/s/cm(2), i.e., distributed over the decade in flux just below the ROSAT All Sky Survey limit. This is sufficiently bright for extensive X-ray follow-up campaigns. Once Planck finds these objects, XMM-Newton and Chandra could measure temperatures to 10% for a sample of similar to 100 clusters in the range 0.5 < z < 1, a valuable increase in the number of massive clusters studied over this range. C1 [Chamballu, A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London NW7 2AZ, England. [Chamballu, A.; Bartlett, J. G.] Univ Paris Diderot, APC, Lab AstroParticule & Cosmol, UMR 7164, F-75205 Paris 13, France. [Bartlett, J. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Melin, J. -B.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. RP Chamballu, A (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London NW7 2AZ, England. EM a.chamballu@imperial.ac.uk NR 64 TC 4 Z9 4 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2012 VL 544 AR A40 DI 10.1051/0004-6361/201015431 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100040 ER PT J AU Dahlburg, RB Einaudi, G Rappazzo, AF Velli, M AF Dahlburg, R. B. Einaudi, G. Rappazzo, A. F. Velli, M. TI Turbulent coronal heating mechanisms: coupling of dynamics and thermodynamics SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; magnetohydrodynamics (MHD); turbulence ID MHD TURBULENCE; SOLAR CORONA; LOOPS; DISSIPATION; FIELDS AB Context. Photospheric motions shuffle the footpoints of the strong axial magnetic field that threads coronal loops, which gives rise to turbulent nonlinear dynamics that are characterized by the continuous formation and dissipation of field-aligned current sheets in which energy is deposited at small-scales and the heating occurs. Previous studies showed that the current sheet thickness is several orders of magnitude smaller than present-day state-of-the-art observational resolution (similar to 700 km). Aims. To understand coronal heating and correctly interpret observations it is crucial to study the thermodynamics of such a system in which energy is deposited at unresolved small-scales. Methods. Fully compressible three-dimensional magnetohydrodynamic simulations were carried out to understand the thermodynamics of coronal heating in the magnetically confined solar corona. Results. We show that temperature is highly structured at scales below observational resolution. It is also nonhomogeneously distributed so that only a fraction of the coronal mass and volume is heated at each time. Conclusions. This is a multi-thermal system in which hotter and cooler plasma strands are also found next to each other at sub-resolution scales and exhibit a temporal dynamics. C1 [Dahlburg, R. B.] USN, Lab Computat Phys & Fluid Dynam, Res Lab, Washington, DC 20375 USA. [Einaudi, G.] Berkeley Res Associates Inc, Beltsville, MD 20705 USA. [Rappazzo, A. F.] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA. [Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dahlburg, RB (reprint author), USN, Lab Computat Phys & Fluid Dynam, Res Lab, Washington, DC 20375 USA. EM rdahlbur@lcp.nrl.navy.mil FU NASA FX This work was carried out in part at the Jet Propulsion Laboratory under a contract with NASA. R. B. D. thanks P. Byrne for helpful conversations. NR 19 TC 21 Z9 21 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2012 VL 544 AR L20 DI 10.1051/0004-6361/201219752 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100180 ER PT J AU Hekker, S Elsworth, Y Mosser, B Kallinger, T Chaplin, WJ De Ridder, J Garcia, RA Stello, D Clarke, BD Hall, JR Ibrahim, KA AF Hekker, S. Elsworth, Y. Mosser, B. Kallinger, T. Chaplin, W. J. De Ridder, J. Garcia, R. A. Stello, D. Clarke, B. D. Hall, J. R. Ibrahim, K. A. TI Solar-like oscillations in red giants observed with Kepler: influence of increased timespan on global oscillation parameters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: oscillations; stars: late-type; stars: interiors; techniques: photometric ID 1ST 4 MONTHS; NGC 6819; MAIN-SEQUENCE; STARS; COROT; ASTEROSEISMOLOGY; AMPLITUDES; MODES; DETECTABILITY; CONSTRAINTS AB Context. The length of the asteroseismic timeseries obtained from the Kepler satellite analysed here span 19 months. Kepler provides the longest continuous timeseries currently available, which calls for a study of the influence of the increased timespan on the accuracy and precision of the obtained results. Aims. We aim to investigate how the increased timespan influences the detectability of the oscillation modes, and the absolute values and uncertainties of the global oscillation parameters, i.e., frequency of maximum oscillation power, nu(max), and large frequency separation between modes of the same degree and consecutive orders, . Methods. We use published methods to derive nu(max) and for timeseries ranging from 50 to 600 days and compare these results as a function of method, timespan and . Results. We find that in general a minimum of the order of 400 day long timeseries are necessary to obtain reliable results for the global oscillation parameters in more than 95% of the stars, but this does depend on . In a statistical sense the quoted uncertainties seem to provide a reasonable indication of the precision of the obtained results in short (50-day) runs, they do however seem to be overestimated for results of longer runs. Furthermore, the different definitions of the global parameters used in the different methods have non-negligible effects on the obtained values. Additionally, we show that there is a correlation between nu(max) and the flux variance. Conclusions. We conclude that longer timeseries improve the likelihood to detect oscillations with automated codes (from similar to 60% in 50 day runs to >95% in 400 day runs with a slight method dependence) and the precision of the obtained global oscillation parameters. The trends suggest that the improvement will continue for even longer timeseries than the 600 days considered here, with a reduction in the median absolute deviation of more than a factor of 10 for an increase in timespan from 50 to 2000 days (the currently foreseen length of the mission). This work shows that global parameters determined with high precision - thus from long datasets - using different definitions can be used to identify the evolutionary state of the stars. C1 [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Hekker, S.; Elsworth, Y.; Chaplin, W. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Mosser, B.] Univ Paris 07, Univ Paris 06, Observ Paris, LESIA,UMR 8109, F-92195 Meudon, France. [Kallinger, T.; De Ridder, J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Garcia, R. A.] Univ Paris 07, IRFU SAp, Ctr Saclay, Lab AIM,CEA,DSM,CNRS, F-91191 Gif Sur Yvette, France. [Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Clarke, B. D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hall, J. R.; Ibrahim, K. A.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hekker, S (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM S.Hekker@uva.nl OI Kallinger, Thomas/0000-0003-3627-2561; Garcia, Rafael/0000-0002-8854-3776 FU NASA's Science Mission Directorate; Netherlands Organisation for Scientific Research (NWO); Science and Technology Facilities Council (STFC) FX Funding for this Discovery Mission is provided by NASA's Science Mission Directorate. The Kepler Team is recognized for helping to make the mission and these data possible. S. H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). Y.E. and W.J.C. acknowledge support from the Science and Technology Facilities Council (STFC). NR 43 TC 21 Z9 21 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 AUG PY 2012 VL 544 AR A90 DI 10.1051/0004-6361/201219328 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100090 ER PT J AU Limousin, M Ebeling, H Richard, J Swinbank, AM Smith, GP Jauzac, M Rodionov, S Ma, CJ Smail, I Edge, AC Jullo, E Kneib, JP AF Limousin, M. Ebeling, H. Richard, J. Swinbank, A. M. Smith, G. P. Jauzac, M. Rodionov, S. Ma, C. -J. Smail, I. Edge, A. C. Jullo, E. Kneib, J. -P. TI Strong lensing by a node of the cosmic web The core of MACS J0717.5+3745 at z=0.55 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: strong; galaxies: clusters: individual: MACS J0717.5+3745; large-scale structure of Universe; dark matter ID DARK-MATTER HALOS; SPACE-TELESCOPE OBSERVATIONS; HIGH-DENSITY ENVIRONMENTS; LUMINOUS GALAXY CLUSTERS; ALL-SKY SURVEY; DISCOVERY; UNIVERSE; DISTANT; Z-GREATER-THAN-0.5; ABELL-1689 AB We present results of a strong-lensing analysis of MACS J0717.5+3745 (here after MACS J0717), an extremely X-ray luminous galaxy cluster at z = 0.55. Observations at different wavelengths reveal a complex and dynamically very active cluster, whose core is connected to a large scale filament extended over several Mpc. Using multi-passband imaging data obtained with the Hubble Space Telescope's Advanced Camera for Surveys (ACS), we identify 15 multiply imaged systems across the full field of view of ACS, five of which we confirmed spectroscopically in ground-based follow-up observations with the Keck telescope. We use these multiply imaged systems to constrain a parametric model of the mass distribution in the cluster core, employing a new parallelized version of the LENSTOOL software. The main result is that the most probable description of the mass distribution comprises four cluster-scale dark matter haloes. The total mass distribution follows the light distribution but strongly deviates from the distribution of the intra-cluster gas as traced by the X-ray surface brightness. This confirms the complex morphology proposed by previous studies. We interpret this segregation of collisional and collisionless matter as strong evidence of multiple mergers and ongoing dynamical activity. MACS J0717 thus constitutes one of the most disturbed clusters presently known and, featuring a projected mass within the ACS field of view (R = 150" = 960 kpc) of 2.11 +/- 0.23 x 10(15) M-circle dot, the system is also one of the most massive known. C1 [Limousin, M.; Jauzac, M.; Rodionov, S.; Jullo, E.; Kneib, J. -P.] Univ Provence, CNRS, Lab Astrophys Marseille, UMR 6610, F-13388 Marseille 13, France. [Limousin, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Richard, J.] Univ Lyon 1, Observ Lyon, CRAL, F-69561 St Genis Laval, France. [Swinbank, A. M.; Smail, I.; Edge, A. C.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Smith, G. P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Smith, G. P.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Jauzac, M.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa. [Ma, C. -J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Ma, C. -J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jullo, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Limousin, M (reprint author), Univ Provence, CNRS, Lab Astrophys Marseille, UMR 6610, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France. EM marceau.limousin@oamp.fr RI Rodionov, Sergey/K-2166-2013; Smail, Ian/M-5161-2013; Jauzac, Mathilde/B-1966-2015; Kneib, Jean-Paul/A-7919-2015; OI Rodionov, Sergey/0000-0002-9661-8221; Smail, Ian/0000-0003-3037-257X; Kneib, Jean-Paul/0000-0002-4616-4989; Edge, Alastair/0000-0002-3398-6916 FU Centre National de la Recherche Scientifique; STScI [GO-09722, GO-10420]; SAO [GO3-4168X]; Danish National Research Foundation FX M. L. thanks Massimo Meneghetti and Adi Zitrin for helpful discussions. M. L. and J. P. K. acknowledge the Centre National de la Recherche Scientifique for its support. H. E. acknowledges financial support from STScI grants GO-09722 and GO-10420 as well as SAO grant GO3-4168X. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work has been conducted using facilities offered by CeSAM (Centre de donneeS Astrophysiques de Marseille, http://lam.oamp.fr/cesam/. NR 40 TC 33 Z9 33 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 AUG PY 2012 VL 544 AR A71 DI 10.1051/0004-6361/201117921 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100071 ER PT J AU Mawet, D Absil, O Montagnier, G Riaud, P Surdej, J Ducourant, C Augereau, JC Rottinger, S Girard, J Krist, J Stapelfeldt, K AF Mawet, D. Absil, O. Montagnier, G. Riaud, P. Surdej, J. Ducourant, C. Augereau, J. -C. Roettinger, S. Girard, J. Krist, J. Stapelfeldt, K. TI Direct imaging of extra-solar planets in star forming regions Lessons learned from a false positive around IM Lupi SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planet-disk interactions; stars: variables: T Tauri, Herbig Ae/Be; planetary systems; stars: individual: IM Lup; infrared: planetary systems; techniques: high angular resolution ID T-TAURI STARS; MAIN-SEQUENCE STARS; BETA-PICTORIS; GIANT PLANET; EVOLUTIONARY MODELS; LINE-PROFILES; BROWN DWARFS; MASS STARS; CATALOG; SPECTRA AB Context. Most exoplanet imagers consist of ground-based adaptive optics coronagraphic cameras which are currently limited in contrast, sensitivity and astrometric precision, but advantageously observe in the near-infrared window (1-5 mu m). Because of these practical limitations, our current observational aim at detecting and characterizing planets puts heavy constraints on target selection, observing strategies, data reduction, and follow-up. Most surveys so far have thus targeted young systems (1-100 Myr) to catch the putative remnant thermal radiation of giant planets, which peaks in the near-infrared. They also favor systems in the solar neighborhood (d < 80 pc), which eases angular resolution requirements but also ensures a good knowledge of the distance and proper motion, which are critical to secure the planet status, and enable subsequent characterization. Aims. Because of their youth, it is very tempting to target the nearby star forming regions, which are typically twice as far as the bulk of objects usually combed for planets by direct imaging. Probing these interesting reservoirs sets additional constraints that we review in this paper by presenting the planet search that we initiated in 2008 around the disk-bearing T Tauri star IM Lup, which is part of the Lupus star forming region (140-190 pc). Methods. We show and discuss why age determination, the choice of evolutionary model for both the central star and the planet, precise knowledge of the host star proper motion, relative or absolute (between different instruments) astrometric accuracy (including plate scale calibration), and patience are the key ingredients for exoplanet searches around more distant young stars. Results. Unfortunately, most of the time, precision and perseverance are not paying off: we discovered a candidate companion around IM Lup in 2008, which we report here to be an unbound background object. We nevertheless review in details the lessons learned from our endeavor, and additionally present the best detection limits ever calculated for IM Lup. We also accessorily report on the successful use of innovative data reduction techniques, such as the damped-LOCI and iterative roll subtraction. C1 [Mawet, D.; Montagnier, G.; Girard, J.] European So Observ, Santiago, Chile. [Mawet, D.; Krist, J.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Absil, O.; Riaud, P.; Surdej, J.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. [Augereau, J. -C.; Roettinger, S.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Ducourant, C.] Univ Bordeaux, LAB, UMR5804, F-33271 Floirac, France. [Stapelfeldt, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mawet, D (reprint author), European So Observ, Alonso de Cordova 3107, Santiago, Chile. EM dmawet@eso.org OI Girard, Julien/0000-0001-8627-0404 FU National Aeronautics and Space Administration (NASA); Communaute francaise de Belgique - Actions de recherche concertees - Academie universitaire Wallonie-Europe; NASA's Astrophysics Data System; SIMBAD database FX This work was carried out at the European Southern Observatory (ESO) site of Vitacura (Santiago, Chile), and the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under contract with the National Aeronautics and Space Administration (NASA). O.A. and J.S. acknowledge support from the Communaute francaise de Belgique - Actions de recherche concertees - Academie universitaire Wallonie-Europe. This research has made use of the NASA/IPAC/NExScI Star and Exoplanet Database, which is operated by the JPL, Caltech, under contract with NASA, and NASA's Astrophysics Data System and of the SIMBAD database, operated at CDS (Strasbourg, France). NR 55 TC 4 Z9 4 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 AUG PY 2012 VL 544 AR A131 DI 10.1051/0004-6361/201219662 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100131 ER PT J AU Meeus, G Montesinos, B Mendigutia, I Kamp, I Thi, WF Eiroa, C Grady, CA Mathews, G Sandell, G Martin-Zaidi, C Brittain, S Dent, WRF Howard, C Menard, F Pinte, C Roberge, A Vandenbussche, B Williams, JP AF Meeus, G. Montesinos, B. Mendigutia, I. Kamp, I. Thi, W. F. Eiroa, C. Grady, C. A. Mathews, G. Sandell, G. Martin-Zaidi, C. Brittain, S. Dent, W. R. F. Howard, C. Menard, F. Pinte, C. Roberge, A. Vandenbussche, B. Williams, J. P. TI Observations of Herbig Ae/Be stars with Herschel/PACS The atomic and molecular contents of their protoplanetary discs SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: identification; astrochemistry; circumstellar matter; planetary systems; protoplanetary disks ID INTERMEDIATE-MASS STARS; MAIN-SEQUENCE STARS; X-RAY-EMISSION; T-TAURI STARS; YOUNG STARS; HD 100546; AEBE STARS; CIRCUMSTELLAR DISKS; ACCRETION RATES; BETA-PICTORIS AB We observed a sample of 20 representative Herbig Ae/Be stars and 5 A-type debris discs with PACS onboard Herschel, as part of the GAS in Protoplanetary Systems (GASPS) project. The observations were done in spectroscopic mode, and cover the far-infrared lines of [OI], [CII], CO, CH+, H2O, and OH. We have a [OI] 63 mu m detection rate of 100% for the Herbig Ae/Be and 0% for the debris discs. The [OI] 145 mu m line is only detected in 25% and CO J = 18-17 in 45% (and fewer cases for higher J transitions) of the Herbig Ae/Be stars, while for [CII] 157 mu m, we often find spatially variable background contamination. We show the first detection of water in a Herbig Ae disc, HD 163296, which has a settled disc. Hydroxyl is detected as well in this disc. First seen in HD 100546, CH+ emission is now detected for the second time in a Herbig Ae star, HD 97048. We report fluxes for each line and use the observations as line diagnostics of the gas properties. Furthermore, we look for correlations between the strength of the emission lines and either the stellar or disc parameters, such as stellar luminosity, ultraviolet and X-ray flux, accretion rate, polycyclic aromatic hydrocarbon (PAH) band strength, and flaring. We find that the stellar ultraviolet flux is the dominant excitation mechanism of [OI] 63 mu m, with the highest line fluxes being found in objects with a large amount of flaring and among the largest PAH strengths. Neither the amount of accretion nor the X-ray luminosity has an influence on the line strength. We find correlations between the line flux of [OI] 63 mu m and [OI] 145 mu m, CO J = 18-17 and [OI] 6300 A, and between the continuum flux at 63 mu m and at 1.3 mm, while we find weak correlations between the line flux of [OI] 63 mu m and the PAH luminosity, the line flux of CO J = 3-2, the continuum flux at 63 mu m, the stellar effective temperature, and the Br gamma luminosity. Finally, we use a combination of the [OI] 63 mu m and (CO)-C-12 J = 2-1 line fluxes to obtain order of magnitude estimates of the disc gas masses, in agreement with the values that we find from detailed modelling of two Herbig Ae/Be stars, HD 163296 and HD 169142. C1 [Meeus, G.; Mendigutia, I.; Eiroa, C.] Univ Autonoma Madrid, Dpt Fis Teor, E-28049 Madrid, Spain. [Montesinos, B.] CAB CSIC INTA, Dept Astrophys, Villanueva De La Canada 28691, Spain. [Kamp, I.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Thi, W. F.; Martin-Zaidi, C.; Menard, F.; Pinte, C.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys IPAG, UMR 5274, F-38041 Grenoble, France. [Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA. [Grady, C. A.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Mathews, G.; Williams, J. P.] Univ Hawaii, Inst Astron IfA, Honolulu, HI 96822 USA. [Sandell, G.; Howard, C.] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brittain, S.] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29634 USA. [Dent, W. R. F.] ALMA SCO, Santiago, Chile. [Roberge, A.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vandenbussche, B.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. RP Meeus, G (reprint author), Univ Autonoma Madrid, Dpt Fis Teor, Campus Cantoblanco, E-28049 Madrid, Spain. EM gwendolyn.meeus@uam.es RI Roberge, Aki/D-2782-2012; Montesinos, Benjamin/C-3493-2017; OI Roberge, Aki/0000-0002-2989-3725; Montesinos, Benjamin/0000-0002-7982-2095; Williams, Jonathan/0000-0001-5058-695X; Mendigutia, Ignacio/0000-0002-0233-5328 FU NASA/JPL; CNES; Millennium Science Initiative (ICM) of the Chilean ministry of Economy [Nucleus P10-022-F]; EU FP7 [284405, PERG06-GA-2009-256513]; ANR of France [ANR-2010-JCJC-0504-01]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI (Italy); CICT/MCT (Spain); [AYA-2008-01727]; [AYA-2011-26202]; [RYC-2011-07920] FX We would like to thank the PACS instrument team for their dedicated support and A. Carmona for discussions about gas line diagnostics. G. Meeus, C. Eiroa, I. Mendigutia, and B. Montesinos are partly supported by AYA-2008-01727 and AYA-2011-26202. G. Meeus is supported by RYC-2011-07920. C.A.G. and S.D.B. acknowledge NASA/JPL for funding support. W.F.T. thanks CNES for financial support. F.M. thanks the Millennium Science Initiative (ICM) of the Chilean ministry of Economy (Nucleus P10-022-F). F.M., I.K., and W.F.T. acknowledge support from the EU FP7-2011 under Grant Agreement No. 284405. C.P. acknowledges funding from the EU FP7 under contract PERG06-GA-2009-256513 and from ANR of France under contract ANR-2010-JCJC-0504-01. 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). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 132 TC 58 Z9 58 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 AUG PY 2012 VL 544 AR A78 DI 10.1051/0004-6361/201219225 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100078 ER PT J AU Pineda, JL Mizuno, N Rollig, M Stutzki, J Kramer, C Klein, U Rubio, M Kawamura, A Minamidani, T Benz, A Burton, M Fukui, Y Koo, BC Onishi, T AF Pineda, J. L. Mizuno, N. Roellig, M. Stutzki, J. Kramer, C. Klein, U. Rubio, M. Kawamura, A. Minamidani, T. Benz, A. Burton, M. Fukui, Y. Koo, B. -C. Onishi, T. TI Submillimeter line emission from LMC 30 Doradus: The impact of a starburst on a low-metallicity environment SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; submillimeter: ISM; galaxies: ISM; ISM: clouds; Magellanic Clouds ID LARGE-MAGELLANIC-CLOUD; PHOTON-DOMINATED REGIONS; GIANT MOLECULAR CLOUDS; PHOTODISSOCIATION REGIONS; INTERSTELLAR-MEDIUM; IRREGULAR GALAXIES; HII-REGIONS; DARK GAS; C-I; CARBON AB Context. The 30 Dor region in the Large Magellanic Cloud (LMC) is the most vigorous star-forming region in the Local Group. Star formation in this region is taking place in low-metallicity molecular gas that is exposed to an extreme far-ultraviolet (FUV) radiation field powered by the massive compact star cluster R136. 30 Dor is therefore ideally suited to study the conditions in which stars formed at earlier cosmological times. Aims. Observations of (sub) mm and far-infrared (FIR) spectral lines of the main carbon-carrying species, CO, [CI] and [CII], which originate in the surface layers of molecular clouds illuminated by the FUV radiation of young stars, can be used to constrain the physical and chemical state of the star-forming ISM. Methods. We used the NANTEN2 telescope to obtain high-angular resolution observations of the (CO)-C-12 J = 4 -> 3, J = 7 -> 6, and (CO)-C-13 J = 4 -> 3 rotational lines and [CI] P-3(1)-P-3(0) and P-3(2)-P-3(1) fine-structure submillimeter transitions in 30 Dor-10, the brightest CO and FIR-emitting cloud at the center of the 30 Dor region. We derived the physical and chemical properties of the low-metallicity molecular gas using an excitation/radiative transfer code and found a self-consistent solution of the chemistry and thermal balance of the gas in the framework of a clumpy cloud PDR model. We compared the derived properties with those in the N159W region, which is exposed to a more moderate far-ultraviolet radiation field compared with 30 Dor-10, but has similar metallicity. We also combined our CO detections with previously observed low-J CO transitions to derive the CO spectral-line energy distribution in 30 Dor-10 and N159W. Results. The separate excitation analysis of the submm CO lines and the neutral carbon fine structure lines shows that the mid-J CO and [CI]-emitting gas in the 30 Dor-10 region has a temperature of about 160K and a H-2 density of about 10(4) cm(-3). We find that the molecular gas in 30 Dor-10 is warmer and has a lower beam filling factor compared to that of N159W, which might be a result of the effect of a strong FUV radiation field heating and disrupting the low-metallicity molecular gas. We use a clumpy PDR model (including the [CII] line intensity reported in the literature) to constrain the FUV intensity to about chi(0) approximate to 3100 and an average total H density of the clump ensemble of about 10(5) cm(-3) in 30 Dor-10. C1 [Pineda, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mizuno, N.; Kawamura, A.] Natl Inst Nat Sci, Natl Astron Observ Japan, ALMA J Project Off, Mitaka, Tokyo 1818588, Japan. [Roellig, M.; Stutzki, J.] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany. [Kramer, C.] Inst Radioastron Milimetr, Granada 18012, Spain. [Klein, U.] Argelander Inst Astron, D-53121 Bonn, Germany. [Rubio, M.] Univ Chile, Dept Astron, Santiago, Chile. [Minamidani, T.] Hokkaido Univ, Dept Phys, Fac Sci, Kita Ku, Sapporo, Hokkaido 0600810, Japan. [Benz, A.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Burton, M.] UNSW, Sch Phys, Sydney, NSW 2052, Australia. [Fukui, Y.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Koo, B. -C.] Seoul Natl Univ, Seoul 151742, South Korea. [Onishi, T.] Osaka Prefecture Univ, Dept Astrophys, Osaka 5998531, Japan. RP Pineda, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Jorge.Pineda@jpl.nasa.gov RI Rubio, Monica/J-3384-2016; OI Minamidani, Tetsuhiro/0000-0001-9778-6692; Burton, Michael/0000-0001-7289-1998 FU FONDECYT(CHILE) [1080335] FX This research was conducted at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. We would like to thank William Langer and Paul Goldsmith for careful reading of the manuscript and enlightening discussions. The NANTEN2 project (southern submillimeter observatory consisting of a 4-m telescope) is based on a mutual agreement between Nagoya University and The University of Chile and includes member universities from six countries, Australia, Republic of Chile, Federal Republic of Germany, Japan, Republic of Korea, and Swiss Confederation. M. R. wishes to acknowledge support from FONDECYT(CHILE) grant 1080335. NR 44 TC 10 Z9 10 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2012 VL 544 AR A84 DI 10.1051/0004-6361/201118321 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100084 ER PT J AU Rousseau, R Grondin, MH Van Etten, A Lemoine-Goumard, M Bogdanov, S Hessels, JWT Kaspi, VM Arzoumanian, Z Camilo, F Casandjian, JM Espinoza, CM Johnston, S Lyne, AG Smith, DA Stappers, BW Caliandro, GA AF Rousseau, R. Grondin, M. -H. Van Etten, A. Lemoine-Goumard, M. Bogdanov, S. Hessels, J. W. T. Kaspi, V. M. Arzoumanian, Z. Camilo, F. Casandjian, J. M. Espinoza, C. M. Johnston, S. Lyne, A. G. Smith, D. A. Stappers, B. W. Caliandro, G. A. TI Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE pulsars: general; pulsars: individual: PSR J1856+0245; ISM: individual objects: HESS J1857+026; gamma rays: general ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; DRIVEN SUPERNOVA-REMNANTS; SPACE-TELESCOPE; EVOLUTION; MODEL; J1825-137; EMISSION; CATALOG; YOUNG AB Context. Since its launch, the Fermi satellite has firmly identified 5 pulsar wind nebulae plus a large number of candidates, all powered by young and energetic pulsars. HESS J1857+026 is a spatially extended gamma-ray source detected by H.E.S.S. and classified as a possible pulsar wind nebula candidate powered by PSR J1856+0245. Aims. We search for gamma-ray pulsations from PSR J1856+0245 and explore the characteristics of its associated pulsar wind nebula. Methods. Using a rotational ephemeris obtained from the Lovell telescope at Jodrell Bank Observatory at 1.5 GHz, we phase-fold 36 months of gamma-ray data acquired by the Large Area Telescope (LAT) aboard Fermi. We also perform a complete gamma-ray spectral and morphological analysis. Results. No gamma-ray pulsations were detected from PSR J1856+0245. However, significant emission is detected at a position coincident with the TeV source HESS J1857+026. The gamma-ray spectrum is well described by a simple power-law with a spectral index of Gamma = 1.53 +/- 0.11(stat) +/- 0.55(syst) and an energy flux of G(0.1-100 GeV) = (2.71 +/- 0.52(stat) +/- 1.51(syst)) x 10(-11) erg cm(-2) s(-1). The gamma-ray luminosity is L-PWN(gamma) (0.1-100 GeV) = (2.5 +/- 0.5(stat) +/- 1.5(syst)) x 10(35) (d/9 kpc)(2) erg s(-1), assuming a distance of 9 kpc. This implies a gamma-ray efficiency of similar to 5% for (E) over bar = 4.6 x 10(36) erg s(-1), in the range expected for pulsar wind nebulae. Detailed multi-wavelength modeling provides new constraints on its pulsar wind nebula nature. C1 [Rousseau, R.; Lemoine-Goumard, M.; Smith, D. A.] Univ Bordeaux 1, CNRS IN2p3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Grondin, M. -H.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Grondin, M. -H.] Univ Heidelberg, Landessternwarte, D-69117 Heidelberg, Germany. [Van Etten, A.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Van Etten, A.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bogdanov, S.; Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hessels, J. W. T.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Hessels, J. W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Kaspi, V. M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Casandjian, J. M.] Univ Paris Diderot, CEA IRFU CNRS, CEA Saclay, Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France. [Espinoza, C. M.; Lyne, A. G.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Johnston, S.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Caliandro, G. A.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. RP Rousseau, R (reprint author), Univ Bordeaux 1, CNRS IN2p3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. EM rousseau@cenbg.in2p3.fr; Marie-Helene.Grondin@mpi-hd.mpg.de; ave@stanford.edu; lemoine@cenbg.in2p3.fr FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization; Japan Aerospace Exploration Agency (JAXA) in Japan; K.A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Science and Technology Facilities Council of the United Kingdom; European Community [ERC-StG-259391] 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 Lovell Telescope is owned and operated by the University of Manchester as part of the Jodrell Bank Centre for Astrophysics with support from the Science and Technology Facilities Council of the United Kingdom.; Funded by contract ERC-StG-259391 from the European Community. NR 42 TC 9 Z9 9 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2012 VL 544 AR A3 DI 10.1051/0004-6361/201118685 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100003 ER PT J AU Telting, JH Ostensen, RH Baran, AS Bloemen, S Reed, MD Oreiro, R Farris, L Ottosen, TA Aerts, C Kawaler, SD Heber, U Prins, S Green, EM Kalomeni, B O'Toole, SJ Mullally, F Sanderfer, DT Smith, JC Kjeldsen, H AF Telting, J. H. Ostensen, R. H. Baran, A. S. Bloemen, S. Reed, M. D. Oreiro, R. Farris, L. Ottosen, T. A. Aerts, C. Kawaler, S. D. Heber, U. Prins, S. Green, E. M. Kalomeni, B. O'Toole, S. J. Mullally, F. Sanderfer, D. T. Smith, J. C. Kjeldsen, H. TI Three ways to solve the orbit of KIC 11 558 725: a 10-day beaming sdB+WD binary with a pulsating subdwarf SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: early-type; binaries: spectroscopic; subdwarfs; stars: oscillations; stars: individual: KIC11558725 ID B-STARS; COMPACT PULSATORS; CLOSE BINARIES; SURVEY PHASE; COMPANIONS; PHOTOMETRY; DISCOVERY; ORIGIN; SYSTEM AB The recently discovered subdwarf B (sdB) pulsator KIC11 558 725 is one of the 16 pulsating sdB stars detected in the Kepler field. It features a rich g-mode frequency spectrum, with a few low-amplitude p-modes at short periods. This makes it a promising target for a seismic study aiming to constrain the internal structure of this star, and of sdB stars in general. We have obtained ground-based spectroscopic radial-velocity measurements of KIC 11 558 725 based on low-resolution spectra in the Balmer-line region, spanning the 2010 and 2011 observing seasons. From these data we have discovered that KIC11 558 725 is a binary with period P = 10.05 d, and that the radial-velocity amplitude of the sdB star is 58 km s(-1). Consequently the companion of the sdB star has a minimum mass of 0.63 M-circle dot, and is therefore most likely an unseen white dwarf. We analyse the near-continuous 2010-2011 Kepler light curve to reveal the orbital Doppler-beaming effect, giving rise to light variations at the 238 ppm level, which is consistent with the observed spectroscopic orbital radial-velocity amplitude of the subdwarf. We use the strongest 70 pulsation frequencies in the Kepler light curve of the subdwarf as clocks to derive a third consistent measurement of the orbital radial-velocity amplitude, from the orbital light-travel delay. The orbital radius a(sdB) sin i = 11.5 R-circle dot gives rise to a light-travel time delay of 53.6 s, which causes aliasing and lowers the amplitudes of the shortest pulsation frequencies, unless the effect is corrected for. We use our high signal-to-noise average spectra to study the atmospheric parameters of the sdB star, deriving T-eff = 27 910K and log g = 5.41 dex, and find that carbon, nitrogen and oxygen are underabundant relative to the solar mixture. Furthermore, we analyse the Kepler light curve for its pulsational content and extract more than 160 significant frequencies. We investigate the pulsation frequencies for expected period spacings and rotational splittings. We find period-spacing sequences of spherical-harmonic degrees l = 1 and l = 2, and we associate a large fraction of the g-modes in KIC 11 558 725 with these sequences. From frequency splittings we conclude that the subdwarf is rotating subsynchronously with respect to the orbit. C1 [Telting, J. H.] Nordic Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Ostensen, R. H.; Bloemen, S.; Aerts, C.; Prins, S.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Baran, A. S.; Reed, M. D.; Farris, L.] Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65804 USA. [Oreiro, R.] Inst Astrofis Andalucia CSIC, Granada 18008, Spain. [Ottosen, T. A.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Aerts, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Heber, U.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte Bamberg, Erlangen, Germany. [Green, E. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kalomeni, B.] Univ Ege, Dept Astron & Space Sci, TR-35100 Izmir, Turkey. [O'Toole, S. J.] Australian Astron Observ, Epping, NSW 1710, Australia. [Mullally, F.; Sanderfer, D. T.; Smith, J. C.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Telting, JH (reprint author), Nordic Opt Telescope, Apartado 474, Santa Cruz De La Palma 38700, Spain. EM jht@not.iac.es RI Heber, Ulrich/G-3306-2013; OI Heber, Ulrich/0000-0001-7798-6769; Amby, Thomas Mellergaard/0000-0002-8116-1097; Oreiro Rey, Raquel/0000-0002-4899-6199; Kawaler, Steven/0000-0002-6536-6367 FU National Science Foundation; Missouri Space Grant Consortium; NASA; NASA's Science Mission Directorate; European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC [227224]; Research Council of KU Leuven grant [GOA/2008/04] FX Based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos (ORM) of the Instituto de Astrofisica de Canarias, and the William Herschel Telescope and Isaac Newton Telescope also at ORM, operated by the Isaac Newton Group. M.D.R. and L.F. were Visiting Astronomers to the Kitt Peak National Observatory, 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. M.D.R. and L.F. were supported by the Missouri Space Grant Consortium funded by NASA. The authors gratefully acknowledge the Kepler team and all who have contributed to enabling the mission. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (prosperity), as well as from the Research Council of KU Leuven grant agreement GOA/2008/04. J.H.T. cordially thanks the Instituut voor Sterrenkunde, KU Leuven, for its hospitality. NR 40 TC 29 Z9 29 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 AUG PY 2012 VL 544 AR A1 DI 10.1051/0004-6361/201219458 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100001 ER PT J AU McFadden, LA Bastien, FA Mutchler, M Crow, CA Weir, H Li, JY Hamilton, DP AF McFadden, Lucy A. Bastien, Fabienne A. Mutchler, Max Crow, Carolyn A. Weir, Heather Li, Jian-Yang Hamilton, Douglas P. TI Upper limits on the size of satellites of Asteroid (4) Vesta from 2007 Hubble Space Telescope observations SO ICARUS LA English DT Article DE Asteroid Vesta; Satellites of asteroids; Hubble Space Telescope observations ID EUCRITES; PLUTO; DAWN AB We imaged the region around Asteroid (4) Vesta in nine long exposures using the Wide Field Planetary Camera 2 on the Hubble Space Telescope on May 14 and 16, 2007 to conduct a deep search for satellites in support of NASA's Dawn mission that orbited (4) Vesta in 2011-2012. Several previous search efforts have been undertaken, but no satellites were detected. Our search covered distances from 14 to 260 Vesta radii and searched to a limiting magnitude of 22.5 +/- 0.4 in HST's wide-band red filter (F702W). Our upper limit for possible satellites corresponds to a satellite just 22 +/- 4 m in radius, assuming the same optical properties as Vesta. Our upper limit is similar to 10 times smaller than the best limit of previous searches. In situ satellite searches by NASA's Dawn spacecraft will probe regions closer to Vesta than our effort reported here. Published by Elsevier Inc. C1 [McFadden, Lucy A.; Bastien, Fabienne A.; Crow, Carolyn A.; Weir, Heather; Li, Jian-Yang; Hamilton, Douglas P.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mutchler, Max] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Weir, Heather] Sci Syst Applicat, Lanham, MD 20706 USA. RP McFadden, LA (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 160, Greenbelt, MD 20771 USA. EM lucy.mcfadden@nasa.gov RI McFadden, Lucy-Ann/I-4902-2013 OI McFadden, Lucy-Ann/0000-0002-0537-9975 FU NASA through Space Telescope Science Institute [GO 10799]; NASA [NAS5-26555]; UCLA [2090SJB692] FX Support for this work was provided by NASA through GO 10799 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA Contract NAS5-26555.; We thank our program coordinator, William Januszewski and staff at Space Telescope Science Institute for making these observations possible. L.A.M. acknowledges partial support for this work by the Dawn Project under contract from UCLA to University of Maryland 2090SJB692. Reviews by Susan Benecchi and Bill Merline were very helpful. NR 33 TC 2 Z9 2 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 AUG PY 2012 VL 220 IS 2 BP 305 EP 310 DI 10.1016/j.icarus.2012.05.002 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200002 ER PT J AU Tornabene, LL Osinski, GR Mcewenb, AS Boyce, JM Bray, VJ Caudill, CM Grant, JA Hamilton, CW Mattson, S Mouginis-Mark, PJ AF Tornabene, Livio L. Osinski, Gordon R. McEwenB, Alfred S. Boyce, Joseph M. Bray, Veronica J. Caudill, Christy M. Grant, John A. Hamilton, Christopher W. Mattson, Sarah Mouginis-Mark, Peter J. TI Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process SO ICARUS LA English DT Article DE Mars, Surface; Cratering; Impact processes; Geological processes; Terrestrial planets ID SCIENCE EXPERIMENT HIRISE; GROUND ICE; EJECTA MORPHOLOGIES; ELYSIUM-PLANITIA; SINUS SABAEUS; DEPOSITS; REGIONS; UTOPIA; ORIGIN; MELT AB Recently acquired high-resolution images of martian impact craters provide further evidence for the interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of craters are nearly equally distributed between the two hemispheres, spanning from 53 degrees S to 62 degrees N latitude. They range in diameter from similar to 1 to 150 km, and are found at elevations between -5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clusters and range in size from similar to 10 m to as large as 3 km. Pit sizes scale with both the host crater's diameter and the host deposit size. These pits have subtle raised rims, and unlike primary and secondary impact craters, they lack well-defined ejecta deposits and overlapping stratigraphic relationships. They also lack any sign of any preferential alignment expected of volcanic or tectonic collapse features. Morphologic and stratigraphic evidence in support of an impact origin includes the observation that pitted materials primarily occur as ponded and flow-like deposits on crater floors, behind terraces, and infilling the lowest local topographic depressions atop the ejecta blanket similar to the distribution of impact melt-bearing bodies on the Moon. Based on the observations and comparisons to terrestrial and lunar analogs, we conclude that the pit-bearing materials are impactite deposits. The presence of these deposits in older craters, where preserved, suggests that they have formed on Mars throughout most of its geologic history; thus, understanding their origin may help to constrain the hydrological and climate history of Mars. (C) 2012 Elsevier Inc. All rights reserved. C1 [Tornabene, Livio L.; Osinski, Gordon R.] Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON N6A 5B7, Canada. [McEwenB, Alfred S.; Bray, Veronica J.; Caudill, Christy M.; Mattson, Sarah] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Boyce, Joseph M.; Mouginis-Mark, Peter J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Manoa, HI 96822 USA. [Grant, John A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Hamilton, Christopher W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tornabene, LL (reprint author), Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON N6A 5B7, Canada. EM ltornabe@uwo.ca FU NASA/JPL MRO project via the HiRISE Science and Operations team; Smithsonian Institution's "Charles Lindbergh" fellowship through the Center for Earth and Planetary Studies; NASA Postdoctoral Program at the Goddard Space Flight Center FX This work was supported by NASA/JPL MRO project via the HiRISE Science and Operations team, and the Smithsonian Institution's "Charles Lindbergh" fellowship through the Center for Earth and Planetary Studies. C.W.H. is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. We would like to personally thank and acknowledge: Guy McArthur (CTX help), Patrick Russell (helpful discussions), the JMARS team, especially Eric Engle who personally helped me troubleshoot various GIS-related issues that were essential to the success of this study, Deanne Daigle who helped edit a final version of this manuscript, and the MRO and LRO, especially HiRISE, CTX and LROC teams, respectively, for all the wonderful crater-related data collected over the last few years. We'd also like to extend a special thanks to Horton Newsom and Seth Kadish for their invaluable time as reviewers and their efforts to help improve this manuscript for publication. NR 104 TC 33 Z9 33 U1 3 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 AUG PY 2012 VL 220 IS 2 BP 348 EP 368 DI 10.1016/j.icarus.2012.05.022 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200006 ER PT J AU Irwin, PGJ de Bergh, C Courtin, R Bezard, B Teanby, NA Davis, GR Fletcher, LN Orton, GS Calcutt, SB Tice, D Hurley, J AF Irwin, P. G. J. de Bergh, C. Courtin, R. Bezard, B. Teanby, N. A. Davis, G. R. Fletcher, L. N. Orton, G. S. Calcutt, S. B. Tice, D. Hurley, J. TI The application of new methane line absorption data to Gemini-N/NIFS and KPNO/FTS observations of Uranus' near-infrared spectrum SO ICARUS LA English DT Article DE Uranus, Atmosphere; Radiative transfer; Atmospheres, Composition ID OCCULTATION MEASUREMENTS; SPECTROSCOPIC DATABASE; PLANETARY ATMOSPHERE; CLOUD STRUCTURE; BAND; H-2; CH4; PARAMETERS; ABUNDANCE; HYDROGEN AB New line data describing the absorption of CH4 and CH3D from 1.26 to 1.71 mu m (Campargue, A., Wang, L. Mondelain, D., Kassi, S., Bezard, B., Lellouch, E., Coustenis, A., de Bergh, C., Hirtzig, M., Drossart, P. [2012]. Icarus 219, 110-128), building upon previous papers by Campargue et al. (Campargue, A., Wang, L, Kassi, S., Masat, M., Votava, O. [2010]. J. Quant. Spectrosc. Radiat. Transfer 111, 1141-1151; Wang, L, Kassi, S., Campargue, A. [2010]. J. Quant. Spectrosc. Radiat. Transfer 111, 1130-1140; Wang, L., Kassi, S., Liu, A.W., Hu, S.M., Campargue, A. [2011]. J. Quant. Spectrosc. Radiat. Transfer 112, 937-951)) have been applied to the analysis of Gemini-N/NIFS observations of Uranus made in 2010 and compared with earlier disc-averaged observations made by KPNO/FTS in 1982. The new line data are found to improve greatly the fit to the observed spectra and present a huge advance over previous methane absorption tables by allowing us to determine the CH3D/CH4 ratio and also start to break the degeneracy between methane abundance and cloud top height. The best fits are obtained if the cloud particles in the main cloud deck at the 2-3 bar level become less scattering with wavelength across the 1.4-1.6 mu m region and we have modelled this variation here by varying the extinction cross-section and single-scattering albedo of the particles. Applying the new line data to the NIFS spectra of Uranus, we determine a new estimate of the CH3D/CH4 ratio of 2.9(-0.5)(+0.9) x 10(-4), which is consistent with the estimate of de Bergh etal. (de Bergh, C., Lutz, B.L., Owen, T., Brault, J., Chauville, J. [1986]. Astrophys. J. 311, 501-510) of 3.6(-2.8)(+3.6) x 10(-4), made by fitting a disc-averaged KPNO/FTS spectrum measured in 1982, but much better constrained. The NIFS observations made in 2010 have been disc-averaged and compared with the 1982 KPNO/FTS spectrum and found to be in excellent agreement. Using k-tables fitted to the new line data, the central meridian observations of Uranus' H-band spectrum (1.49-1.64 mu m) made by Gemini-N/NIFS in 2010 have been reanalyzed. The use of the new methane absorption coefficients and the modified scattering properties of the cloud particles in the main cloud deck appears to break the degeneracy between cloud height and methane abundance immediately above it in this spectral region and we find that both vary with latitude across Uranus' disc. Overall, we find that the main cloud deck becomes higher, but thinner from equator to poles, with a local maximum in cloud top height in the circumpolar zones at 45 degrees N and 45 degrees S. At the same time, using the 'D' temperature pressure profile of Lindal et al. (Lindal, G.F., Lyons, J.R., Sweetnam, D.N., Eshleman, V.R., Hinson, D.P. [1987]. J. Geophys. Res. 92, 14987-15001) and a deep methane abundance of 1.6% (Baines, K.H., Mickelson, ME., Larson, LE., Ferguson, D.W. [1995]. Icarus 144, 328-340) we find that the relative humidity of methane is high near the equator (similar to 60%) and decreases sharply towards the poles, except near the circumpolar zone at 45 degrees N, which has brightened steadily since 2007, and where there is a local maximum in methane relative humidity. In tests conducted with the warmer 'F1' profile of Sromovsky et al. (2011) we find a similar variation of methane abundance above the main cloud, although for this warmer temperature profile this abundance is dependent mostly on the fitted deep methane mole fraction. (C) 2012 Elsevier Inc. All rights reserved. C1 [Irwin, P. G. J.; Fletcher, L. N.; Calcutt, S. B.; Tice, D.; Hurley, J.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [de Bergh, C.; Courtin, R.; Bezard, B.] Univ Paris 07, Univ Paris 06, Observ Paris, LESIA,UMR CNRS 8109, F-92195 Meudon, France. [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Davis, G. R.] Joint Astron Ctr, Hilo, HI 96720 USA. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Irwin, PGJ (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England. EM irwin@atm.ox.ac.uk RI Fletcher, Leigh/D-6093-2011; OI Fletcher, Leigh/0000-0001-5834-9588; Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X FU United Kingdom Science and Technology Facilities Council; Leverhulme Trust; University of Oxford; NASA; French "Agence Nationale de la Recherche" (ANR) FX We are grateful to the United Kingdom Science and Technology Facilities Council for funding this research and also to our support astronomers: Richard McDermid (2009, 2010), Chad Trujillo (2009, 2010), Andy Adamson (2007, 2008), Watson Varricattu (2006), and also to Ilona Soechting and Andrew Gosling in the UK Gemini Office. Nicholas Teanby acknowledges the support of the Leverhulme Trust. Leigh Fletcher was supported by a Glasstone fellowship at the University of Oxford. Glenn Orton was supported by a grant from NASA to the jet Propulsion Laboratory, California Institute of Technology. Catherine de Bergh, Regis Courtin and Bruno Bezard acknowledge the financial support from the French "Agence Nationale de la Recherche" (ANR project: CH4@Titan). The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. NR 34 TC 26 Z9 26 U1 0 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 AUG PY 2012 VL 220 IS 2 BP 369 EP 382 DI 10.1016/j.icarus.2012.05.017 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200007 ER PT J AU Cloutis, EA Hudon, P Hiroi, T Gaffey, MJ Mann, P AF Cloutis, E. A. Hudon, P. Hiroi, T. Gaffey, M. J. Mann, P. TI Spectral reflectance properties of carbonaceous chondrites-5: CO chondrites SO ICARUS LA English DT Article DE Asteroids, Composition; Mineralogy; Meteorites; Spectroscopy ID ISOLATED OLIVINE GRAINS; ISOTOPIC COMPOSITIONS; ORGANIC-MATTER; THERMAL HISTORIES; RICH INCLUSIONS; CM CHONDRITES; PARENT-BODY; METEORITES; SPECTROSCOPY; ASTEROIDS AB We examined the spectral reflectance properties of 16 CO-type carbonaceous chondrites (CCs) in order to better understand their range of spectral properties, develop spectral-compositional correlations, and provide information that may aid in the search for CO parent bodies. As a group, our CO powder spectra have some similarities and differences. COs have experienced varying degree of thermal metamorphism, with petrologic subgrades ranging from similar to CO3.0 to similar to CO3.8. Their reflectance spectra are characterized by a ubiquitous absorption feature in the 1 mu m region, and a nearly ubiquitous feature in the 2 mu m region that appears in CO >3.1 spectra. The 1 mu m region feature is attributable to abundant Fe-bearing amorphous phases (and Fe-poor olivine) in the lower petrologic subtypes, which gradually transforms to more abundant and Fe-rich olivine with increasing metamorphism. The increase in depth and decrease in wavelength position of this feature are consistent with this transformation. All but the least-altered COs also exhibit an absorption feature in the 2 mu m region whose depth also generally increases with increasing metamorphic grade, resulting in increasingly blue-sloped spectra and larger band area ratios. The wavelength position and change in depth of this feature (ranging from 0% to 12.2%) is consistent with increasing Fe2+ in spinel, which is present in calcium-aluminum and ameboid olivine inclusions. Reflectance of a local reflectance maximum near 0.8 mu m increases with increasing thermal metamorphism and this is likely due to the loss and aggregation of carbonaceous phases. The increasing reflectance is negatively correlated with various measures of spectral slope (i.e., brighter = bluer), and while this cannot be uniquely attributed to any one cause, it is consistent with increasing spinel Fe2+ content and decreasing carbonaceous material abundance or aggregation. With decreasing grain size. CO spectra normally become brighter and more red-sloped. The 0.6/0.5 mu m ratios of CO falls are consistently higher than CO finds, suggesting that terrestrial weathering has affected the visible wavelength region spectral properties of finds. Unmetamorphosed CO spectra may be difficult to distinguish from the least altered CM chondrites. However above petrologic grade similar to 3.1, COs can be uniquely discriminated from Cl, CM, metamorphosed Cl and CM, and CR chondrites, by the presence of both olivine and spinel absorption bands. Some K-class asteroids exhibit olivine and spinel absorption bands, consistent with CO chondrites, although modeled olivine:spinel ratios are generally lower in these asteroids than in CO chondrites. (C) 2012 Elsevier Inc. All rights reserved. C1 [Cloutis, E. A.; Mann, P.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Hudon, P.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Off, Houston, TX 77058 USA. [Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada. EM e.cloutis@uwinnipeg.ca; pierre.hudon@mcgill.ca; takahiro_hiroi@brown.edu; gaffey@space.edu FU NASA [NNG06GJ31G]; NSERC FX We wish to thank the invaluable and generous assistance provided by many individuals which made this study possible. In particular we thank the US and Japanese Antarctic meteorite programs for recovering the majority of the samples included in this study. The RELAB facility at Brown University is a multi-user facility operated with support from NASA Planetary Geology and Geophysics Grant NNG06GJ31G, whose support is gratefully acknowledged. This study was supported by an NSERC Discovery grant to EAC. We also thank the two anonymous reviewers for their insightful comments and suggestions. NR 119 TC 12 Z9 12 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 466 EP 486 DI 10.1016/j.icarus.2012.05.019 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200014 ER PT J AU Cloutis, EA Hudon, P Hiroi, T Gaffey, MJ AF Cloutis, E. A. Hudon, P. Hiroi, T. Gaffey, M. J. TI Spectral reflectance properties of carbonaceous chondrites 4: Aqueously altered and thermally metamorphosed meteorites SO ICARUS LA English DT Article DE Meteorites; Asteroids, Surfaces; Asteroids, Composition; Spectroscopy ID MACROMOLECULAR ORGANIC-MATTER; CM CHONDRITES; ABSORPTION-BANDS; SOLAR-SYSTEM; SPECTROSCOPY; ASTEROIDS; MINERALS; MARS; SOIL; YAMATO-793321 AB We examined the spectral reflectance properties of 26 carbonaceous chondrites (CCs) that show evidence of aqueous alteration and subsequent thermal metamorphism (termed ATCCs). We also reviewed the thermal and aqueous alteration history of these meteorites and searched for trends between spectral parameters and temperature histories in order to uncover spectral-compositional relationships. Aqueous alteration results in the production of phyllosilicates from anhydrous silicate precursors - largely serpentine group phyllosilicates, and increasing amounts of saponite group phyllosilicates with increasing aqueous alteration. Thermal metamorphism results in dehydration of these phyllosilicates and production of abundant amorphous material except at the highest temperatures (greater than or similar to 900 degrees C), as well as alteration of carbonaceous components. ATCCs are a spectrally diverse group in almost all respects. Spectral slopes, as measured by the ratio of reflectance at 2.4 mu m to the local peak or inflection in the 0.5-0.8 mu m region and 2.4/1.5 mu m ratios range from 0.78 to 1.48, and 0.93 to 1.24, respectively (blue-sloped spectra have ratio values of <1). ATCC powder spectra (<75, <100, or <125 mu m) are generally dark, with maximum reflectance at the local peak or inflection in the 0.5-0.8 mu m region, or maximum reflectance at any wavelength ranging from 2.6% to 8.9%, and 3.5% to 10.3%, respectively. All ATCC spectra exhibit an absorption feature in the similar to 0.8-1.3 mu m region, with band depths ranging from similar to 1% to 8%. This feature is diverse in terms of number of apparent absorption bands. The presence of mixed valence Fe2+-Fe3+ phyllosilicates, as evidenced by an absorption band near 0.7 mu m with a depth of up to 5%, and Mg-bearing phyllosilicates, as evidenced by an MgOH combination band in the 2.3-2.4 mu m region, are seen in many of the least thermally metamorphosed ATCC spectra. The depth of the 0.7 mu m band generally decreases with increasing temperature. Olivine-associated absorption bands in the 0.8-1.3 mu m region seem to be more prevalent in the more metamorphosed ATCC spectra. However clearly-resolvable olivine absorption bands are not present in ATCC spectra, suggesting that thermal metamorphism did not lead to the production of widespread crystalline Fe2+-bearing olivine. The reddest ATCC powder spectra are generally the darkest, and C content is correlated with decreasing overall reflectance and weakly correlated with spectral slope. When the degree of thermal metamorphism was compared to various spectral measures of slope, band depth, and overall reflectance, no strong correlations emerged. However, it does appear that the most thermally metamorphosed ATCCs have generally flatter spectral slopes. ATCC chip spectra are brighter and less red-sloped than powder spectra, but band depths are generally comparable. Laboratory-heated Cls and CMs generally exhibit the same types of spectral changes seen in naturally thermally metamorphosed ATCCs. For laboratory-heated CM and Cl chondrites, and ATCCs for which temperature estimates are available, reflectance generally decreases with increasing temperature to similar to 500 degrees C, and then increases to higher temperatures. Silicate absorption band depths are generally least for temperatures of similar to 600-800 degrees T. Below this temperature interval, ATCC spectra show more phyllosilicate-like absorption bands. ATCC spectra generally become flatter with increasing temperature above similar to 400 degrees C. Temperatures in excess of those experienced by the ATCCs (similar to 900 degrees C) are required for the appearance of well-resolved olivine absorption bands. (C) 2012 Elsevier Inc. All rights reserved. C1 [Cloutis, E. A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Hudon, P.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Off, Houston, TX 77058 USA. [Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada. EM e.cloutis@uwinnipeg.ca; pierre.hudon@mcgill.ca; takahiro_hiroi@brown.edu; gaffey@space.edu FU NASA [NNG06GJ31G]; NSERC FX We wish to thank the invaluable and generous assistance provided by many individuals which made this study possible. In particular we thank the US and Japanese Antarctic meteorite programs for recovering the majority of the samples included in this study. The RELAB facility at Brown University is a multi-user facility operated with support from NASA Planetary Geology and Geophysics Grant NNG06GJ31G, whose support is gratefully acknowledged. This study was supported by an NSERC Discovery Grant to E.A.C. We also wish to thank Beth Clark and Faith Vilas for their insightful reviews. NR 108 TC 19 Z9 19 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 AUG PY 2012 VL 220 IS 2 BP 586 EP 617 DI 10.1016/j.icarus.2012.05.018 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200022 ER PT J AU Gerakines, PA Hudson, RL Moore, MH Bell, JL AF Gerakines, Perry A. Hudson, Reggie L. Moore, Marla H. Bell, Jan-Luca TI In situ measurements of the radiation stability of amino acids at 15-140 K SO ICARUS LA English DT Article DE Astrobiology; Cosmochemistry; Ices, IR spectroscopy ID ULTRAVIOLET PHOTOLYSIS; ETHYLENE-GLYCOL; L-ALANINE; PARAMAGNETIC-RESONANCE; LABORATORY EXPERIMENTS; VIBRATIONAL ANALYSIS; ORGANIC-MOLECULES; INFRARED-SPECTRA; ION IRRADIATION; L-PHENYLALANINE AB We present new kinetics data on the radiolytic destruction of amino acids measured in situ with infrared spectroscopy. Samples were irradiated at 15, 100, and 140 K with 0.8-MeV protons, and amino-acid decay was followed at each temperature with and without H2O present. Observed radiation products included CO2 and amines, consistent with amino-acid decarboxylation. The half-lives of glycine, alanine, and phenylalanine were estimated for various extraterrestrial environments. Infrared spectral changes demonstrated the conversion from the non-zwitterion structure NH2-CH2(R)-COOH at 15 K to the zwitterion structure +NH3-CH2(R)-COO- at 140 K for each amino acid studied. Published by Elsevier Inc. C1 [Gerakines, Perry A.; Hudson, Reggie L.; Moore, Marla H.; Bell, Jan-Luca] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Gerakines, PA (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 661, Greenbelt, MD 20771 USA. EM perry.a.gerakines@nasa.gov RI Gerakines, Perry/D-2226-2012 OI Gerakines, Perry/0000-0002-9667-5904 FU NASA Astrobiology Institute (NAI); Goddard Center for Astrobiology (GCA); NASA's Exobiology Program FX Zan Peeters constructed and tested the sublimation oven for amino acids. The authors wish to acknowledge support from the NASA Astrobiology Institute (NAI) and the Goddard Center for Astrobiology (GCA), particularly for the summer research internship of JLB. The support of NASA's Exobiology Program is gratefully acknowledged. In addition, we thank Steve Brown, Tom Ward, and Eugene Gerashchenko, members of the Radiation Effects Facility at NASA Goddard Space Flight Center, for operation of the proton accelerator. NR 58 TC 19 Z9 19 U1 1 U2 27 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 647 EP 659 DI 10.1016/j.icarus.2012.06.001 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200026 ER PT J AU Soderblom, JM Barnes, JW Soderblom, LA Brown, RH Griffith, CA Nicholson, PD Stephan, K Jaumann, R Sotin, C Baines, KH Buratti, BJ Clark, RN AF Soderblom, Jason M. Barnes, Jason W. Soderblom, Laurence A. Brown, Robert H. Griffith, Caitlin A. Nicholson, Philip D. Stephan, Katrin Jaumann, Ralf Sotin, Christophe Baines, Kevin H. Buratti, Bonnie J. Clark, Roger N. TI Modeling specular reflections from hydrocarbon lakes on Titan SO ICARUS LA English DT Article DE Titan; Saturn, Satellites; Satellites, Surfaces; Satellites, Atmospheres; Infrared observations ID LIQUID; ETHANE; METHANE; SURFACE; ATMOSPHERE; RADIOMETER; DESCENT; RADAR AB During the 58th close flyby of Titan (T58), the Cassini Visual and Infrared Mapping Spectrometer (VIMS) observed a specular reflection of sunlight from Titan's Jingpo Lacus through the 5-mu m methane window (Stephan, K. et al. [2010]. Geophys. Res. Lett. 37, L07104). The maximum intensity of this reflection is controlled by three basic factors: (1) the shape of the reflecting surface (its overall geometry and roughness), (2) the reflectance of the surface, as controlled by the real refractive index of the material (and that of the atmosphere), and (3) attenuation due to absorption and scattering by atmospheric gases and aerosols along the pathlength. Herein we model the expected intensity of a specular reflection off of a convex mirror-like surface on Titan. We assume the specular reflection is from a body of liquid hydrocarbons on Titan's surface with optical properties consistent with CH4 and C2H6 with smaller amounts of nitrogen and heavier hydrocarbons (e.g., C3H8) admixed. We assume the 5-mu m opacity for the polar atmosphere is a factor of two higher than that of the tropical haze. For the geometry of the T58 observations, our model predicts a maximum I/F = 1-to-5; for a Lambertian surface at normal illumination I/F = 1. The maximum 5-mu m intensity observed during T58 was I/F similar to 2.6, from which we conclude that Jingpo Lacus is filled with a liquid that has a real index of refraction consistent with that of methane-ethane-nitrogen liquid and that the 5-mu m atmospheric opacity was tau = 0.5, consistent with the higher particle column expected in the winter polar atmosphere. Future VIMS observations will allow us to refine the refractive index of the liquid in the lakes and to place a quantitative constraint on the ratio of methane to ethane. (C) 2012 Elsevier Inc. All rights reserved. C1 [Soderblom, Jason M.; Brown, Robert H.; Griffith, Caitlin A.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Soderblom, Laurence A.] US Geol Survey, Flagstaff, AZ 86001 USA. [Nicholson, Philip D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Stephan, Katrin; Jaumann, Ralf] Inst Planetary Res, DLR, Berlin, Germany. [Jaumann, Ralf] Free Univ Berlin, Inst Geosci, Dept Earth Sci, Berlin, Germany. [Sotin, Christophe; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sotin, Christophe] Univ Nantes, Lab Planetol & Geodynam, Nantes 03, France. [Baines, Kevin H.] Univ Wisconsin, SSEC, Madison, WI 53706 USA. [Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA. RP Soderblom, JM (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM jms4@mit.edu RI Barnes, Jason/B-1284-2009; OI Barnes, Jason/0000-0002-7755-3530; Soderblom, Jason/0000-0003-3715-6407 FU Cassini Project; NASA FX We wish to thank to the VIMS operations group as well as the entire Cassini project for their tremendous efforts delivering Cassini to Saturn and obtaining and returning these data. We thank Peter Gierasch for providing calculations of refraction in Titan's atmosphere. We thank Ralph Lorenz and an anonymous reviewer for their helpful review of this manuscript. This work was supported by the Cassini Project, managed by the Jet Propulsion Laboratory, California Institute of Technology and under contract with NASA NR 28 TC 13 Z9 13 U1 0 U2 21 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 744 EP 751 DI 10.1016/j.icarus.2012.05.030 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200032 ER PT J AU Dalton, JB Cruikshank, DP Clark, RN AF Dalton, J. Brad, III Cruikshank, Dale P. Clark, Roger N. TI Compositional analysis of Hyperion with the Cassini Visual and Infrared Mapping Spectrometer SO ICARUS LA English DT Article DE Infrared observations; Saturn, Satellites; Regoliths ID REFLECTANCE SPECTROSCOPY; AROMATIC-HYDROCARBONS; SPECTRAL PROPERTIES; IAPETUS; PHOEBE; HYDROGEN; DUST; SATELLITES; COMETARY; ORGANICS AB Compositional mapping of the surface of Hyperion using Cassini Visual and Infrared Mapping Spectrometer (VIMS) observations reveals a heterogeneous surface dominated by water ice accompanied by additional materials. Carbon dioxide, as evidenced by a prominent absorption band centered at 4.26 mu m, is distributed over most of the surface, including icy regions. This does not represent exposures of pure CO2 ice, but concentrations of CO2 molecules adsorbed on other materials or complexed in H2O, perhaps as a clathrate (Cruikshank, D.P., Meyer, A.W., Brown, R.H., Clark, R.N., Jaumann, R., Stephan, K., Hibbitts, CA., Sandford, S.A., Mastrapa, R., Filacchione, G., Dalle Ore, CM., Nicholson, P.D., Buratti, B.J., McCord, T.B., Nelson, R.M., Dalton, J.B., Baines, K.H., Matson, D.L., The VIMS Team [2010]. Icarus 206, 561-572). Localized deposits of low-albedo material in subcircular depressions exhibit spectral absorptions indicative of C-H in aromatic (3.29 mu m) and aliphatic (3.35-3.50 mu m) hydrocarbons. An absorption band at 2.42 mu m that is also seen on other saturnian satellites, tentatively identified as H-2 (Clark, R.N. et al. [2011]. In: Proc. AAS-DPS Meeting, 43, 1563; Clark et al., in preparation, 2012) adsorbed on dark material grains, is also prominent. Our best spectral models included H2O and CO2 ice, with small amounts of nanophase Fe and Fe2O3. Weaker and more spatially scattered absorption features are also found at 4.48, 4.60, and 4.89 mu m, although no clear molecular identifications have yet been made. While strongest in the low-albedo deposits, the CO2, hydrocarbon and putative H-2 bands vary in strength throughout the icy regions, as do the 4.48-, 4.60- and 4.89-mu m bands, suggesting that this background ice is laced with a complex mixture of non-ice compounds. (C) 2012 Elsevier Inc. All rights reserved. C1 [Dalton, J. Brad, III] CALTECH, Jet Prop Lab, Planetary Ices Grp, Pasadena, CA 91109 USA. [Cruikshank, Dale P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Clark, Roger N.] US Geol Survey, Denver, CO 80220 USA. RP Dalton, JB (reprint author), CALTECH, Jet Prop Lab, Planetary Ices Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dalton@jpl.nasa.gov FU National Aeronautics and Space Administration; Cassini Data Analysis Program (CDAP) FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, and NASA Ames Research Center under a contract with the National Aeronautics and Space Administration, and funded through the Cassini Data Analysis Program (CDAP). Cruikshank and Clark are supported in part as co-investigators on the Cassini VIMS team. NR 49 TC 5 Z9 6 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 752 EP 776 DI 10.1016/j.icarus.2012.05.003 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200033 ER PT J AU Rivera-Valentin, EG Blackburn, DG Ulrich, RK AF Rivera-Valentin, Edgard G. Blackburn, David G. Ulrich, Richard K. TI Exploring the effects of overburden on the sublimation and transport of H2O on Iapetus SO ICARUS LA English DT Article DE Iapetus; Saturn, Satellites; Satellites, Surfaces ID WATER ICE; ALBEDO DICHOTOMY; ASTROPHYSICAL IMPLICATIONS; SURFACE-PROPERTIES; VAPOR-PRESSURE; DARK MATERIAL; SOLAR-SYSTEM; GAS; SATELLITES; PHOEBE AB It has been shown through both measurements and simulations that there exists a measurable ice-free, porous, overburden overlaying water ice on Cassini Regio. Mass transfer through this porous media in a vacuum would occur in the Knudsen regime, which provides sublimation rates orders of magnitude smaller than Hertz-Langmuir sublimation. The availability of water ice for transport from this region is thus currently controlled by mass transfer through the dark material overburden. Thermal segregation suggests that Iapetus' polar regions have been brightened via ballistic transport of water and its subsequent cold trapping since exogenic deposition models predict dark high latitudes on the leading hemisphere. The limiting effect of the dark material on transport of water ice may thus greatly impact the current mass balance at the poles. The effects of the overburden on the global stability and transport of H2O is addressed in order to gain insight into its influence on the polar albedo distribution and current state of thermal segregation within the dark terrain. Results indicate that thermal segregation is currently an inactive or weak process within Cassini Regio, though it is an ongoing process at the inter-terrain regions. Modeling of polar accumulation suggests that even accounting for the current dark material cover within Cassini Regio there exists sufficient ballistically inbound water to overcome exogenic darkening mechanisms. Topographic effects on local albedo differences are also simulated to provide a more complete water stability study of Iapetus. Results suggest that topographically induced changes in heat flux may be sufficient to create the observed local albedo contrasts and also support ongoing dark exogenic deposition within Cassini Regio to explain the lack of bright slopes deep within the dark terrain. (C) 2012 Elsevier Inc. All rights reserved. C1 [Rivera-Valentin, Edgard G.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. [Blackburn, David G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ulrich, Richard K.] Univ Arkansas, Dept Chem Engn, Fayetteville, AR 72701 USA. RP Rivera-Valentin, EG (reprint author), Univ Arkansas, Arkansas Ctr Space & Planetary Sci, 202 Field House Bldg, Fayetteville, AR 72701 USA. EM egrv314@gmail.com OI Rivera-Valentin, Edgard/0000-0002-4042-003X FU NASA's Planetary Geology and Geophysics; National Aeronautics and Space Administration; NASA; National Science Foundation [0963249, 0959124, 0918970]; Arkansas Science and Technology Authority FX A portion of this work was conducted at the Lunar and Planetary Institute (LPI) where it was supported by a grant from NASA's Planetary Geology and Geophysics and also at the Jet Propulsion Laboratory, California Institute of Technology, under contract of the National Aeronautics and Space Administration where it was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. The modeling portion of this work was partially supported by the National Science Foundation under Grants ARI #0963249, MRI #0959124 (Razor), EPS #0918970 (CI TRAIN), and a grant from the Arkansas Science and Technology Authority, managed by the Arkansas High Performance Computing Center. The authors would also like to thank Dr. Paul Schenk of the LPI for use of his topography maps of Iapetus and image database. The authors would also like to thank the reviewers who helped enhance this manuscript. NR 53 TC 0 Z9 0 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 808 EP 820 DI 10.1016/j.icarus.2012.06.024 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200036 ER PT J AU Jackiewicz, J Nettelmann, N Marley, M Fortney, J AF Jackiewicz, Jason Nettelmann, Nadine Marley, Mark Fortney, Jonathan TI Forward and inverse modeling for jovian seismology SO ICARUS LA English DT Article DE Jupiter; Jupiter, interior; Planetary formation; Abundances, Interiors ID GLOBAL OSCILLATIONS; GIANT PLANETS; JUPITER; SATURN; EQUATION; STATE; TROPOSPHERE; INTERIORS; HYDROGEN; WAVES AB Jupiter is expected to pulsate in a spectrum of acoustic modes and recent re-analysis of a spectroscopic time series has identified a regular pattern in the spacing of the frequencies (Gaulme, P., Schmider, F.-X., Gay, J., Guillot, T., Jacob, C. [2011]. Astron. Astrophys. 531, A104). This exciting result can provide constraints on gross jovian properties and warrants a more in-depth theoretical study of the seismic structure of Jupiter. With current instrumentation, such as the SYMPA instrument (Schmider, F.X. [2007]. Astron. Astrophys. 474, 1073-1080) used for the Gaulme et al. (Gaulme, P., Schmider, F.-X., Gay, J., Guillot, T., Jacob, C. [2011]. Astron. Astrophys. 531, A104) analysis, we assume that, at minimum, a set of global frequencies extending up to angular degree l = 25 could be observed. In order to identify which modes would best constraining models of Jupiter's interior and thus help motivate the next generation of observations, we explore the sensitivity of derived parameters to this mode set. Three different models of the jovian interior are computed and the theoretical pulsation spectrum from these models for l <= 25 is obtained. We compute sensitivity kernels and perform linear inversions to infer details of the expected discontinuities in the profiles in the jovian interior. We find that the amplitude of the sound-speed jump of a few percent in the inner/outer envelope boundary seen in two of the applied models should be reasonably inferred with these particular modes. Near the core boundary where models predict large density discontinuities, the location of such features can be accurately measured, while their amplitudes have more uncertainty. These results suggest that this mode set would be sufficient to infer the radial location and strength of expected discontinuities in Jupiter's interior, and place strong constraints on the core size and mass. We encourage new observations to detect these jovian oscillations. (C) 2012 Elsevier Inc. All rights reserved. C1 [Jackiewicz, Jason] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Nettelmann, Nadine] Univ Rostock, Inst Phys, D-18051 Rostock, Germany. [Marley, Mark] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Jackiewicz, J (reprint author), New Mexico State Univ, Dept Astron, POB 30001,MSC 4500, Las Cruces, NM 88003 USA. EM jasonj@nmsu.edu RI Marley, Mark/I-4704-2013; OI Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943 FU NASA FX We thank Patrick Gaulme for very useful comments about the paper, and acknowledge the suggestions by two anonymous referees that made the text significantly clearer. This work was supported by the NASA Outer Planets Research Program. NR 37 TC 4 Z9 4 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 844 EP 854 DI 10.1016/j.icarus.2012.06.028 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200038 ER PT J AU Cottini, V Nixon, CA Jennings, DE Anderson, CM Gorius, N Bjoraker, GL Coustenis, A Teanby, NA Achterberg, RK Bezard, B de Kok, R Lellouch, E Irwin, PGJ Flasar, FM Bampasidis, G AF Cottini, V. Nixon, C. A. Jennings, D. E. Anderson, C. M. Gorius, N. Bjoraker, G. L. Coustenis, A. Teanby, N. A. Achterberg, R. K. Bezard, B. de Kok, R. Lellouch, E. Irwin, P. G. J. Flasar, F. M. Bampasidis, G. TI Water vapor in Titan's stratosphere from Cassini CIRS far-infrared spectra SO ICARUS LA English DT Article DE Spectroscopy; Atmospheres, Composition; Satellites, Atmospheres; Titan ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; MOLECULAR SPECTROSCOPIC DATABASE; RADIATIVE-TRANSFER; CARBON-MONOXIDE; ATMOSPHERE; PAIRS; SPECTROMETER; TEMPERATURES; AEROSOLS; 300-K AB Here we report the measurement of water vapor in Titan's stratosphere using the Cassini Composite Infrared Spectrometer (CIRS, Flasar, F.M. et al. [2004]. Space Sci. Rev. 115, 169-297). CIRS senses water emissions in the far infrared spectral region near 50 mu m, which we have modeled using two independent radiative transfer codes (NEMESIS (Irwin, P.G.J. et al. [2008]. J. Quant. Spectrosc. Radiat. Trans. 109, 1136-1150) and ART (Coustenis, A. et al. [2007]. Icarus 189, 35-62; Coustenis, A. et al. [2010]. Icarus 207, 461-476). From the analysis of nadir spectra we have derived a mixing ratio of 0.14 +/- 0.05 ppb at an altitude of 97 km, which corresponds to an integrated (from 0 to 600 km) surface normalized column abundance of 3.7 +/- 1.3 x 10(14) molecules/cm(2). In the latitude range 80 degrees S to 30 degrees N we see no evidence for latitudinal variations in these abundances within the error bars. Using limb observations, we obtained mixing ratios of 0.13 +/- 0.04 ppb at an altitude of 115 km and 0.45 +/- 0.15 ppb at an altitude of 230 km, confirming that the water abundance has a positive vertical gradient as predicted by photochemical models (e.g. Lara, L.M., Lellouch, F., Lopez-Moreno, J.J., Rodrigo, R. [1996]. J. Geophys. Res. 101(23), 261; Wilson, E.H., Atreya, S.K. [2004]. J. Geophys. Res. 109, E6; Horst, S.M., Vuitton, V., Yelle, R.V. [2008]. J. Geophys. Res., 113, E10). We have also fitted our data using scaling factors of similar to 0.1-0.6 to these photochemical model profiles, indicating that the models over-predict the water abundance in Titan's lower stratosphere. (C) 2012 Elsevier Inc. All rights reserved. C1 [Cottini, V.; Nixon, C. A.; Jennings, D. E.; Anderson, C. M.; Gorius, N.; Bjoraker, G. L.; Achterberg, R. K.; Flasar, F. M.] NASA, GSFC, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Nixon, C. A.; Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gorius, N.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Coustenis, A.; Lellouch, E.; Bampasidis, G.] Univ Paris Diderot, UPMC Univ Paris 06, CNRS, LESIA Observ Paris, Paris, France. [Coustenis, A.; Lellouch, E.; Bampasidis, G.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [de Kok, R.] SRON, NL-3584 CA Utrecht, Netherlands. [Irwin, P. G. J.] Univ Oxford, Oxford OX1 3PU, England. [Bampasidis, G.] Univ Athens, Fac Phys, Athens 11528, Greece. RP Cottini, V (reprint author), NASA, GSFC, Planetary Syst Lab, Code 693,Bldg 34,Rm S121,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM valeria.cottini@nasa.gov RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Anderson, Carrie/C-8097-2012; OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X FU NASA; NASA Cassini Mission; Leverhulme Trust; UK Science and Technology Facilities Council FX Valeria Cottini is supported by the NASA Postdoctoral Program. Thanks to S. Horst, E. Wilson and S. Atreya for providing their photochemical water profiles for comparison, and to Paul Romani for water chemistry discussions. The US-based authors were funded by the NASA Cassini Mission during the period in which this work was performed. N. Teanby was supported by the Leverhulme Trust and the UK Science and Technology Facilities Council. NR 49 TC 20 Z9 20 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 AUG PY 2012 VL 220 IS 2 BP 855 EP 862 DI 10.1016/j.icarus.2012.06.014 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200039 ER PT J AU Hurford, TA Helfenstein, P Spitale, JN AF Hurford, T. A. Helfenstein, P. Spitale, J. N. TI Tidal control of jet eruptions on Enceladus as observed by Cassini ISS between 2005 and 2007 SO ICARUS LA English DT Article DE Enceladus; Geological processes; Volcanism ID NONSYNCHRONOUS ROTATION; EUROPA; STRESSES AB Observations of Enceladus have revealed active jets of material erupting from cracks on its south polar surface. It has previously been proposed that diurnal tidal stress, driven by Enceladus' orbital eccentricity, may actively produce surface movement along these cracks daily and thus may regulate when eruptions occur. Our analysis of the stress on jet source regions identified in Cassini ISS images reveals tidal stress as a plausible controlling mechanism of jet activity. However, the evidence available in the published and preliminary observations of jet activity between 2005 and 2007 may not be able to solidify the link between tidal stress and eruptions from fissures. Ongoing, far more comprehensive analyses based on recent, much higher resolution jetting observations have the potential to prove otherwise. Published by Elsevier Inc. C1 [Hurford, T. A.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Helfenstein, P.] Cornell Univ, CRSR, Ithaca, NY 14853 USA. [Spitale, J. N.] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Hurford, TA (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 661, Greenbelt, MD 20771 USA. EM terry.a.hurford@nasa.gov RI Hurford, Terry/F-2625-2012 FU NASA FX The authors would like to thank Dr. Richard Greenberg and Dr. Alyssa Rhoden for their thoughtful suggestions, which greatly benefitted this research. This work was supported by NASA Grants issued through the Cassini Data Analysis Program. NR 20 TC 11 Z9 11 U1 1 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 896 EP 903 DI 10.1016/j.icarus.2012.06.022 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200043 ER PT J AU Nicholson, WL McCoy, LE Kerney, KR Ming, DW Golden, DC Schuerger, AC AF Nicholson, Wayne L. McCoy, Lashelle E. Kerney, Krystal R. Ming, Douglas W. Golden, D. C. Schuerger, Andrew C. TI Aqueous extracts of a Mars analogue regolith that mimics the Phoenix landing site do not inhibit spore germination or growth of model spacecraft contaminants Bacillus subtilis 168 and Bacillus pumilus SAFR-032 SO ICARUS LA English DT Article DE Astrobiology; Mars, Surface; Regoliths; Search for extraterrestrial life ID MARTIAN SOIL; ASSEMBLY FACILITY; NITROGEN-CYCLE; TEICHOIC-ACID; UV RESISTANCE; PERCHLORATE; REDUCTION; DISSOLUTION; DIVERSITY; CHEMISTRY AB Because Mars is a primary target for life detection and habitability assessment missions, its exploration is also by necessity a Planetary Protection issue. The recent finding of significant levels of perchlorate (ClO4-) in regolith sampled from the Phoenix landing site raises the question of its potential biotoxicity to putative indigenous martian life, microbial forward contaminants from Earth, or future human visitors. To address this issue, an analogue regolith was constructed based on regolith chemistry data from the Phoenix landing site. A Mars Aqueous Regolith Extract (MARE) was prepared from the Phoenix analogue regolith and analyzed by ion chromatography. The MARE contained (mg/L) the cations Na+ (1411 +/- 181), Mg2+ (1051 +/- 160), Ca2+ (832 +/- 125), and K+ (261 +/- 29), and the anions SO42- (5911 +/- 993), ClO4- (5316 +/- 1767), Cl- (171 +/- 25) and F- (2.0 +/- 0.4). Nitrogen-containing species NO3- (773 +/- 113) and NO2- (6.9 +/- 2.3) were also present as a result of regolith preparation procedures, but their relevance to Mars is at present unknown. The MARE was tested for potential toxic effects on two model spacecraft contaminants, the spore-forming bacteria Bacillus subtilis strain 168 and Bacillus pumilus strain SAFR-032. In B. subtilis, spore germination and initial vegetative growth (up to similar to 5 h) was not inhibited in a rich complex medium prepared with the MARE, but growth after 5 h was significantly suppressed in medium prepared using the MARE. Both B. subtilis and B. pumilus exhibited significantly higher rates of spore germination and growth in the MARE vs. DW with no additions (likely due to endogenous spore nutrients), but germination and growth was further stimulated by addition of glucose and a combination of buffered inorganic salts (K2HPO4, KH2PO4, (NH4)(2)SO4, and MgSO4). The data indicate that the aqueous environment in the regolith from the Phoenix landing site containing high levels of perchlorate does not pose a significant barrier to growth of putative forward contaminants such as B. subtilis and B. pumilus under Earth laboratory conditions. (C) 2012 Elsevier Inc. All rights reserved. C1 [Nicholson, Wayne L.; Kerney, Krystal R.] Univ Florida, Space Life Sci Lab, Dept Microbiol & Cell Sci, Kennedy Space Ctr, FL 32899 USA. [McCoy, Lashelle E.] ESC Team QNA, Qinetiq N Amer Engn Serv Contract, Kennedy Space Ctr, FL 32899 USA. [Ming, Douglas W.] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. [Golden, D. C.] NASA, Johnson Space Ctr, ESCG, Houston, TX 77058 USA. [Schuerger, Andrew C.] Univ Florida, Space Life Sci Lab, Dept Plant Pathol, Kennedy Space Ctr, FL 32899 USA. RP Nicholson, WL (reprint author), Univ Florida, Space Life Sci Lab, Dept Microbiol & Cell Sci, Bldg M6-1025,Room 201-B, Kennedy Space Ctr, FL 32899 USA. EM WLN@ufl.edu; lashelle.e.mccoy@nasa.gov; krystalkerney@ufl.edu; douglas.w.ming@nasa.gov; d.c.golden@nasa.gov; schuerg@ufl.edu OI Kerney, Krystal/0000-0003-4134-0020 FU NASA Planetary Protection office [NNZ08AQ81A, NNH07ZDA001N] FX The authors thank Matthew Pasek, Cassie Conley, and Lanfang Levine for helpful discussions, and the anonymous reviewers for their insightful comments. This work was funded in part by grants from the NASA Planetary Protection office (NNZ08AQ81A and NNH07ZDA001N). NR 58 TC 7 Z9 7 U1 0 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 904 EP 910 DI 10.1016/j.icarus.2012.06.033 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200044 ER PT J AU Hendrix, AR Cassidy, TA Buratti, BJ Paranicas, C Hansen, CJ Teolis, B Roussos, E Bradley, ET Kollmann, P Johnson, RE AF Hendrix, Amanda R. Cassidy, Timothy A. Buratti, Bonnie J. Paranicas, Chris Hansen, Candice J. Teolis, Ben Roussos, Elias Bradley, E. Todd Kollmann, Peter Johnson, Robert E. TI Mimas' far-UV albedo: Spatial variations SO ICARUS LA English DT Article DE Satellites, Composition; Ices, UV spectroscopy; Saturn, Satellites; Ultraviolet observations; Satellites, Surfaces ID HYDROGEN-PEROXIDE; WATER ICE; E-RING; SATURNIAN SATELLITES; ION IRRADIATION; ENCELADUS; PHOTOMETRY; EUROPA; ORIGIN; PHOTOLYSIS AB We present Cassini Ultraviolet Imaging Spectrograph (UVIS) observations of Mimas at far-ultraviolet wavelengths (170-190 nm) which show an interesting albedo gradient across the anti-saturnian hemisphere. We discuss the photometric behavior of Mimas in the far-UV and review the important exogenic processes and their expected effects, relevant over a wide range of wavelengths. We suggest that the UVIS images display the brightening effects of E-ring grain accretion on Mimas' trailing hemisphere; we also show VIMS results that are consistent with E-ring grain accretion on the trailing hemisphere. The UVIS results also suggest the presence of hydrogen peroxide, predominantly in the southern hemisphere, produced by photolysis; this is expected to be a seasonal effect as a result of enhanced UV insolation during the recently-ended southern summer. (C) 2012 Elsevier Inc. All rights reserved. C1 [Hendrix, Amanda R.; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cassidy, Timothy A.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Paranicas, Chris] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Hansen, Candice J.] Planetary Sci Inst, Ivins, UT 84738 USA. [Teolis, Ben] SW Res Inst, San Antonio, TX 78238 USA. [Roussos, Elias; Kollmann, Peter] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Bradley, E. Todd] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Johnson, Robert E.] Univ Virginia, Charlottesville, VA 22904 USA. RP Hendrix, AR (reprint author), CALTECH, Jet Prop Lab, Mail Stop 230-205, Pasadena, CA 91109 USA. EM arh@jpl.nasa.gov RI Paranicas, Christopher/B-1470-2016; Kollmann, Peter/C-2583-2016; OI Paranicas, Christopher/0000-0002-4391-8255; Kollmann, Peter/0000-0002-4274-9760; Roussos, Elias/0000-0002-5699-0678 FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Thanks to Alain Jouchoux and the UVIS operations team at LASP for making these observations happen. We are grateful to John Spencer, Matt Hedman, Joe Burns, Michael Kokorowski, Josh Colwell, Bob West and Greg Holsclaw for helpful suggestions and ideas, and to Marty Snow for providing solar spectra. NR 47 TC 5 Z9 5 U1 1 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 922 EP 931 DI 10.1016/j.icarus.2012.06.012 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200046 ER PT J AU Filacchione, G Capaccioni, F Ciarniello, M Clark, RN Cuzzi, JN Nicholson, PD Cruikshank, DP Hedman, MM Buratti, BJ Lunine, JI Soderblom, LA Tosi, F Cerroni, P Brown, RH McCord, TB Jaumann, R Stephan, K Baines, KH Flamini, E AF Filacchione, G. Capaccioni, F. Ciarniello, M. Clark, R. N. Cuzzi, J. N. Nicholson, P. D. Cruikshank, D. P. Hedman, M. M. Buratti, B. J. Lunine, J. I. Soderblom, L. A. Tosi, F. Cerroni, P. Brown, R. H. McCord, T. B. Jaumann, R. Stephan, K. Baines, K. H. Flamini, E. TI Saturn's icy satellites and rings investigated by Cassini-VIMS: III - Radial compositional variability SO ICARUS LA English DT Article DE Saturn, Satellites; Saturn, Rings; Spectroscopy; Ices ID INFRARED MAPPING SPECTROMETER; OPTICAL-CONSTANTS; MU-M; CRYSTALLINE H2O-ICE; SURFACE-COMPOSITION; ENCELADUS SURFACE; DARK MATERIAL; IAPETUS; PHOEBE; RHEA AB In the last few years Cassini-VIMS, the Visible and Infrared Mapping Spectrometer, returned to us a comprehensive view of the Saturn's icy satellites and rings. After having analyzed the satellites' spectral properties (Filacchione, G., Capaccioni, F., McCord, T.B., Coradini, A., Cerroni, P., Bellucci, G., Tosi, F., D'Aversa, E., Formisano, V., Brown, R.H., Baines, K.H., Bibring, J.P., Buratti, B.J., Clark, R.N., Combes, M., Cruikshank, D.P., Drossart, P., Jaumann, R., Langevin, Y., Matson, D.L., Mennella, V., Nelson, R.M., Nicholson, P.D., Sicardy, B., Sotin, C., Hansen, G., Hibbitts, K., Showalter, M., Newman, S. [2007]. Icarus 186, 259-290, paper I) and their distribution across the satellites' hemispheres (Filacchione, G., Capaccioni, F., Clark, R.N., Cuzzi, J.N., Cruikshank, D.P., Coradini, A., Cerroni, P., Nicholson, P.D., McCord, T.B., Brown, R.H., Buratti, B.J., Tosi, F., Nelson, R.M., Jaumann, R., Stephan, K. [2010]. Icarus 206, 507-523, paper II), we proceed in this paper to investigate the radial variability of icy satellites (principal and minor) and main rings average spectral properties. This analysis is done by using 2264 disk-integrated observations of the satellites and a 12 x 700 pixels-wide rings radial mosaic acquired with a spatial resolution of about 125 km/pixel. Using different VIS and IR spectral indicators, e.g. spectral slopes and band depths, we perform a comparative analysis of these data aimed to measure the distribution of water ice and red contaminant materials across Saturn's system. The average surface regolith grain sizes are estimated with different indicators through comparison with laboratory and synthetic spectra. These measurements highlight very striking differences in the population here analyzed, which vary from the almost uncontaminated and water ice-rich surfaces of Enceladus and Calypso to the metal/organic-rich and red surfaces of Iapetus' leading hemisphere and Phoebe. Rings spectra appear more red than the icy satellites in the visible range but show more intense 1.5-2.0 mu m band depths. Although their orbits are close to the F-ring, Prometheus and Pandora are different in surface composition: Prometheus in fact appears very water ice-rich but at the same time very red at VIS wavelengths. These properties make it very similar to A-B ring particles while Pandora is bluer. Moving outwards, we see the effects of E ring particles, generated by Enceladus plumes, which contaminate satellites surfaces from Mimas out to Rhea. We found some differences between Tethys lagrangian moons, Calypso being much more water ice-rich and bluer than Telesto. Among outer satellites (Hyperion, Iapetus and Phoebe) we observe a linear trend in both water ice decrease and in reddening. Hyperion being the reddest object of the population. The correlations among spectral slopes, band depths, visual albedo and phase permit us to cluster the saturnian population in different spectral classes which are detected not only among the principal satellites and rings but among co-orbital minor moons as well. These bodies are effectively the "connection" elements, both in term of composition and evolution, between the principal satellites and main rings. Finally, we have applied Hapke's theory to retrieve the best spectral fits to Saturn's inner regular satellites (from Mimas to Dione) using the same methodology applied previously for Rhea data discussed in Ciarniello et al. (Ciarniello, M., Capaccioni, F., Filacchione, G., Clark, R.N., Cruikshank, D.P., Cerroni, P., Coradini, A., Brown, R.H., Buratti, B.J., Tosi, F. , Stephan, K. [2011]. Icarus 214, 541-555). (c) 2012 Elsevier Inc. All rights reserved. C1 [Filacchione, G.; Capaccioni, F.; Ciarniello, M.; Tosi, F.; Cerroni, P.] INAF IAPS, Ist Astrofis & Planetol Spaziali, Area Ric Tor Vergata, I-00133 Rome, Italy. [Clark, R. N.] US Geol Survey, Fed Ctr, Denver, CO 80228 USA. [Cuzzi, J. N.; Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nicholson, P. D.; Hedman, M. M.; Lunine, J. I.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Buratti, B. J.; Brown, R. H.; Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Soderblom, L. A.] US Geol Survey, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Flamini, E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Flamini, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McCord, T. B.] Bear Fight Ctr, Winthrop, WA 98862 USA. [Jaumann, R.; Stephan, K.] DLR, Inst Planetary Explorat, D-12489 Berlin, Germany. [Flamini, E.] Agenzia Spaziale Italiana, ASI, I-00198 Rome, Italy. RP Filacchione, G (reprint author), INAF IAPS, Ist Astrofis & Planetol Spaziali, Area Ric Tor Vergata, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM gianrico.filacchione@iaps.inaf.it OI Ciarniello, Mauro/0000-0002-7498-5207; Enrico, Flamini/0000-0001-9521-1705; Cerroni, Priscilla/0000-0003-0239-2741; Capaccioni, Fabrizio/0000-0003-1631-4314; Filacchione, Gianrico/0000-0001-9567-0055; Tosi, Federico/0000-0003-4002-2434 FU Italian Space Agency [I/015/09/0]; NASA through the Cassini project FX This paper is dedicated to the memory of our colleague and friend Angioletta Coradini recently passed away who has inspired us to complete this work. The authors thank VIMS technical team at Lunar and Planetary Lab (University of Arizona, Tucson, AZ), the Cassini-Huygens Project, including engineering and operational teams, at JPL (Pasadena, CA) for the hard work and dedication demonstrated during the entire mission. We gratefully thank the Cassini Icy Satellites and Rings Working groups for their unvaluable comments, observations planning and sequencing. Without all them this study would be impossible. Finally we thank the two anonymous referees which have helped us to improve greatly this paper. This research has made use of NASA's Astrophysics Data System and was completed thanks to the financial support of the Italian Space Agency (Grant I/015/09/0) and NASA through the Cassini project. NR 80 TC 28 Z9 28 U1 1 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2012 VL 220 IS 2 BP 1064 EP 1096 DI 10.1016/j.icarus.2012.06.040 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200056 ER PT J AU Nguyen, HD Miller, IA AF Nguyen, Hien D. Miller, Iain A. TI Cost Impact of Automated Acceptance Testing of Electrical Ground Support Equipment for Spacecraft Testing SO IEEE INSTRUMENTATION & MEASUREMENT MAGAZINE LA English DT Article C1 [Nguyen, Hien D.; Miller, Iain A.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA. [Miller, Iain A.] NASA, Goddard Space Flight Ctr, Washington, DC USA. RP Nguyen, HD (reprint author), Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA. EM Hien.Nguyen@jhuapl.edu; iawmiller@gmail.com NR 4 TC 0 Z9 0 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1094-6969 J9 IEEE INSTRU MEAS MAG JI IEEE Instrum. Meas. Mag. PD AUG PY 2012 VL 15 IS 4 BP 28 EP 33 DI 10.1109/MIM.2012.6263981 PG 6 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 993EE UT WOS:000307837800005 ER PT J AU Cullens, ED Ranzani, L Vanhille, KJ Grossman, EN Ehsan, N Popovic, Z AF Cullens, Evan D. Ranzani, Leonardo Vanhille, Kenneth J. Grossman, Erich N. Ehsan, Negar Popovic, Zoya TI Micro-Fabricated 130-180 GHz Frequency Scanning Waveguide Arrays SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Beam steering; g-band; linear antenna arrays; millimeter wave radar ID MU-COAXIAL LINES; DESIGN AB This paper describes frequency scanning slot arrays operating from 130 to 180 GHz. The arrays are micro-fabricated using the PolyStrata sequential copper deposition process. Measured reflection coefficient and radiation patterns agree with HFSS full-wave simulations. The voltage standing wave ratio is less than 1.75:1 over the entire frequency range, and the measured scanning is 1.04 degrees GHz from 130 to 150 GHz and 32.5 degrees over the full frequency range. The measured gain is 15.5 dBi for a 10-element array at 150 GHz and 18.9 dBi for a 20-element array at 150 GHz with about 3 dB of variation over the scan range. C1 [Cullens, Evan D.; Ranzani, Leonardo; Popovic, Zoya] Univ Colorado, Dept Elect & Comp Engn, Boulder, CO 80309 USA. [Vanhille, Kenneth J.] Nuvotronics LLC, Radford, VA 24141 USA. [Grossman, Erich N.] NIST, Boulder, CO 80303 USA. [Ehsan, Negar] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cullens, ED (reprint author), Univ Colorado, Dept Elect & Comp Engn, Boulder, CO 80309 USA. EM evan.cullens@colorado.edu RI Ranzani, Leonardo/E-8421-2013 FU National Aeronautics and Space Administration (NASA) [NNX10CA77C] FX This work was supported by the National Aeronautics and Space Administration (NASA) under Contract NNX10CA77C. NR 35 TC 21 Z9 21 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-926X EI 1558-2221 J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD AUG PY 2012 VL 60 IS 8 BP 3647 EP 3653 DI 10.1109/TAP.2012.2201089 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 001BW UT WOS:000308435800012 ER PT J AU Esqueda, IS Barnaby, HJ Adell, PC AF Esqueda, Ivan S. Barnaby, Hugh J. Adell, Philippe C. TI Modeling the Effects of Hydrogen on the Mechanisms of Dose Rate Sensitivity SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT Conference on Radiation Effects on Components and Systems (RADECS)/Radiation Effects Data Workshop CY SEP 19-23, 2011 CL Univ Sevilla, Escuela Super Ingenieros, Seville, SPAIN SP Inst Nacl Tecnica Aeroespacial (INTA), Univ Sevilla, Thales Alenia Space, ALTER Technol Grp, ESA, NASA, JPL (NASA/Cal Tech), RADECS Org, IEEE, Nucl & Plasma Sci Soc (NPSS) HO Univ Sevilla, Escuela Super Ingenieros DE Bipolar; dose rate; ELDRS; hydrogen; interface traps; metal-oxide-semiconductor (MOS); silicon dioxide; total ionizing dose (TID) ID GATE MOS DEVICES; BIPOLAR-TRANSISTORS; INTERFACE STATES; RADIATION; IRRADIATION; DEGRADATION; POLYSILICON; BEHAVIOR; OXIDES; ELDRS AB The effects of hydrogen on dose-rate sensitivity are simulated using a one-dimensional (1-D) model that incorporates the physical mechanisms contributing to dose-rate effects in the metal-oxide-semiconductor (MOS) system of gated lateral pnp (GLPNP) bipolar transistors. Calculations show that molecular hydrogen cracking at positively charged defects may be a key reaction relating hydrogen and dose rate response. Comparison to experimental data on bipolar devices is in good agreement with the dose rate calculations of interface trap buildup. C1 [Esqueda, Ivan S.; Barnaby, Hugh J.] Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA. [Adell, Philippe C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Esqueda, IS (reprint author), Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA. EM ivans@asu.edu; hbarnaby@asu.edu; philippe.c.adell@jpl.nasa.gov NR 20 TC 9 Z9 9 U1 0 U2 7 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 AUG PY 2012 VL 59 IS 4 BP 701 EP 706 DI 10.1109/TNS.2012.2195201 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 993XQ UT WOS:000307893700004 ER PT J AU Buchner, S Roche, N Warner, J McMorrow, D Miller, F Morand, S Pouget, V Larue, C Ferlet-Cavrois, V El Mamouni, F Kettunen, H Adell, P Allen, G Aveline, D AF Buchner, S. Roche, N. Warner, J. McMorrow, D. Miller, F. Morand, S. Pouget, V. Larue, C. Ferlet-Cavrois, V. El Mamouni, F. Kettunen, H. Adell, P. Allen, G. Aveline, D. TI Comparison of Single Event Transients Generated at Four Pulsed-Laser Test Facilities-NRL, IMS, EADS, JPL SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT Conference on Radiation Effects on Components and Systems (RADECS)/Radiation Effects Data Workshop CY SEP 19-23, 2011 CL Univ Sevilla, Escuela Super Ingenieros, Seville, SPAIN SP Inst Nacl Tecnica Aeroespacial (INTA), Univ Sevilla, Thales Alenia Space, ALTER Technol Grp, ESA, NASA, JPL (NASA/Cal Tech), RADECS Org, IEEE, Nucl & Plasma Sci Soc (NPSS) HO Univ Sevilla, Escuela Super Ingenieros DE Heavy ions; operational amplifier; photodiode; pulsed laser; single event transients; wavelength ID INTEGRATED-CIRCUITS; CHARGE COLLECTION; LIGHT AB Four pulsed-laser single-event effects systems, differing in wavelength and pulse width, were used to generate single event transients in a large-area silicon photodiode and an operational amplifier (LM124) to determine how transient amplitude and charge collection varied among the different systems. The optical wavelength and the focused spot size are the primary factors influencing the resultant charge density profile. In the large-area photodiode the transients can be distorted by high charge-injection densities that occur for tightly focused, higher energy optical pulses. When the incident laser-pulse energies are corrected for reflection losses and photon efficiency, with collection depth as a floating parameter (to account for diffusion), the photodiode data for all four devices lie on a single curve. The LM124 response varies with the specific transistor irradiated; similar transient shapes are measured for the different pulse wavelengths, with some deviations in the case of R1. These results reiterate that there is no single, optimum pulsed-laser system for SEE studies; that choice depends on the device to be tested, the intended application of that device, the goals of the test, and availability. For the specific devices evaluated here, any of the four laser systems would be sufficient for most tests. C1 [Buchner, S.; Roche, N.; Warner, J.; McMorrow, D.] USN, Res Lab, Washington, DC 20375 USA. [Miller, F.; Morand, S.] EADS France, Suresnes, France. [Pouget, V.; Larue, C.] IMS, Bordeaux, France. [Ferlet-Cavrois, V.] European Space Agcy, ESA ESTEC, NL-2200 AG Noordwijk, Netherlands. [El Mamouni, F.] Vanderbilt Univ, Nashville, TN 37235 USA. [Kettunen, H.] Univ Jyvaskyla, Dept Phys, Accelerator Lab, FI-40014 Jyvaskyla, Finland. [Adell, P.; Allen, G.; Aveline, D.] NASA JPL, Pasadena, CA 91109 USA. RP Buchner, S (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM florent.miller@EADS.net; vincent.pouget@ims-bordeaux.fr; veronique.ferlet-cavrois@esa.int; farah.el.mamouni@vanderbild.edu; Philippe.Adell@jpl.nasa.gov NR 10 TC 10 Z9 10 U1 0 U2 5 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 AUG PY 2012 VL 59 IS 4 BP 988 EP 998 DI 10.1109/TNS.2012.2201956 PN 1 PG 11 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 993XQ UT WOS:000307893700045 ER PT J AU Xapsos, MA Stauffer, CA Jordan, TM Adams, JH Dietrich, WF AF Xapsos, Michael A. Stauffer, Craig A. Jordan, Thomas M. Adams, James H., Jr. Dietrich, William F. TI Periods of High Intensity Solar Proton Flux SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT Conference on Radiation Effects on Components and Systems (RADECS)/Radiation Effects Data Workshop CY SEP 19-23, 2011 CL Univ Sevilla, Escuela Super Ingenieros, Seville, SPAIN SP Inst Nacl Tecnica Aeroespacial (INTA), Univ Sevilla, Thales Alenia Space, ALTER Technol Grp, ESA, NASA, JPL (NASA/Cal Tech), RADECS Org, IEEE, Nucl & Plasma Sci Soc (NPSS) HO Univ Sevilla, Escuela Super Ingenieros DE Solar particle event; worst case flux ID PROBABILITY MODEL; EVENT FLUENCES; PEAK FLUXES; PARTICLES AB Analysis is presented for times during a space mission that specified solar proton flux levels are exceeded. This includes both total time and continuous time periods during missions. Results for the solar maximum and solar minimum phases of the solar cycle are presented and compared for a broad range of proton energies and shielding levels. This type of approach is more amenable to reliability analysis for spacecraft systems and instrumentation than standard statistical models. C1 [Xapsos, Michael A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stauffer, Craig A.] MEI Technol, Seabrook, MD 20706 USA. [Jordan, Thomas M.] EMPC, Gaithersburg, MD 20885 USA. [Adams, James H., Jr.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Dietrich, William F.] USN, Res Lab, Washington, DC 20375 USA. RP Xapsos, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM michael.a.xapsos@nasa.gov NR 19 TC 2 Z9 2 U1 0 U2 5 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 AUG PY 2012 VL 59 IS 4 BP 1054 EP 1059 DI 10.1109/TNS.2012.2196447 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 993XQ UT WOS:000307893700054 ER PT J AU Schwank, JR Shaneyfelt, MR Ferlet-Cavrois, V Dodd, PE Blackmore, EW Pellish, JA Rodbell, KP Heidel, DF Marshall, PW LaBel, KA Gouker, PM Tam, N Wong, R Wen, SJ Reed, RA Dalton, SM Swanson, SE AF Schwank, James R. Shaneyfelt, Marty R. Ferlet-Cavrois, Veronique Dodd, Paul E. Blackmore, Ewart W. Pellish, Jonathan A. Rodbell, Kenneth P. Heidel, David F. Marshall, Paul W. LaBel, Kenneth A. Gouker, Pascale M. Tam, Nelson Wong, Richard Wen, Shi-Jie Reed, Robert A. Dalton, Scott M. Swanson, Scot E. TI Hardness Assurance Testing for Proton Direct Ionization Effects SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT Conference on Radiation Effects on Components and Systems (RADECS)/Radiation Effects Data Workshop CY SEP 19-23, 2011 CL Univ Sevilla, Escuela Super Ingenieros, Seville, SPAIN SP Inst Nacl Tecnica Aeroespacial (INTA), Univ Sevilla, Thales Alenia Space, ALTER Technol Grp, ESA, NASA, JPL (NASA/Cal Tech), RADECS Org, IEEE, Nucl & Plasma Sci Soc (NPSS) HO Univ Sevilla, Escuela Super Ingenieros DE Hardness assurance testing; proton direct ionization effects; single-event upset ID SINGLE-EVENT-UPSETS; NM SOI SRAM; ENERGY AB The potential for using the degraded beam of high-energy proton radiation sources for proton hardness assurance testing for ICs that are sensitive to proton direct ionization effects are explored. SRAMs were irradiated using high energy proton radiation sources (similar to 67 - 70 MeV). The proton energy was degraded using plastic or Al degraders. Peaks in the SEU cross section due to direct ionization were observed. To best observe proton direct ionization effects, one needs to maximize the number of protons in the energy spectrum below the proton energy SEU threshold. SRIM simulations show that there is a tradeoff between increasing the fraction of protons in the energy spectrum with low energies by decreasing the peak energy and the reduction in the total number of protons as protons are stopped in the device as the proton energy is decreased. Two possible methods for increasing the number of low energy protons is to decrease the primary proton energy to reduce the amount of energy straggle and to place the degrader close to the DUT to minimize angular dispersion. These results suggest that high-energy proton radiation sources may be useful for identifying devices sensitive to proton direct ionization. C1 [Schwank, James R.; Shaneyfelt, Marty R.; Dodd, Paul E.; Dalton, Scott M.; Swanson, Scot E.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Ferlet-Cavrois, Veronique] ESA ESTEC, NL-2200 AG Noordwijk, Netherlands. [Blackmore, Ewart W.] TRIUMF, Vancouver, BC V6T 2A3, Canada. [Pellish, Jonathan A.; LaBel, Kenneth A.] NASA, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA. [Rodbell, Kenneth P.; Heidel, David F.] IBM TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Marshall, Paul W.] NASA, Brookneal, VA 24528 USA. [Gouker, Pascale M.] MIT, Lincoln Lab, Lexington, MA 02420 USA. [Tam, Nelson] Marvell, Santa Clara, CA 95054 USA. [Wong, Richard; Wen, Shi-Jie] Cisco Syst, San Jose, CA 95134 USA. [Reed, Robert A.] Vanderbilt Univ, Nashville, TN 37203 USA. RP Schwank, JR (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. EM schwanjr@sandia.gov; shaneymr@sandia.gov; Veronique.Ferlet-Cavrois@esa.int; pedodd@sandia.gov; ewb@triumf.ca; jonathan.a.pellish@nasa.gov; rodbell@us.ibm.com; heidel@us.ibm.com; pwmar-shall@aol.com; ken.label@nasa.gov; pgouker@ll.mit.edu; smdalton@sandia.gov; swansose@sandia.gov NR 11 TC 10 Z9 10 U1 0 U2 7 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 AUG PY 2012 VL 59 IS 4 BP 1197 EP 1202 DI 10.1109/TNS.2011.2177862 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 993XQ UT WOS:000307893700074 ER PT J AU Capossela, KM Brill, RW Fabrizio, MC Bushnell, PG AF Capossela, K. M. Brill, R. W. Fabrizio, M. C. Bushnell, P. G. TI Metabolic and cardiorespiratory responses of summer flounder Paralichthys dentatus to hypoxia at two temperatures SO JOURNAL OF FISH BIOLOGY LA English DT Article DE gill ventilation; heart rate; oxygen extraction; stopflow respirometry AB To quantify the tolerance of summer flounder Paralichthys dentatus to episodic hypoxia, resting metabolic rate, oxygen extraction, gill ventilation and heart rate were measured during acute progressive hypoxia at the fish's acclimation temperature (22 degrees C) and after an acute temperature increase (to 30 degrees C). Mean +/- s.e. critical oxygen levels (i.e. the oxygen levels below which fish could not maintain aerobic metabolism) increased significantly from 27 +/- 2% saturation (2.0 +/- 0.1 mg O2 l-1) at 22 degrees C to 39 +/- 2% saturation (2.4 +/- 0.1 mg O2 l-1) at 30 degrees C. Gill ventilation and oxygen extraction changed immediately with the onset of hypoxia at both temperatures. The fractional increase in gill ventilation (from normoxia to the lowest oxygen level tested) was much larger at 22 degrees C (6.4-fold) than at 30 degrees C (2.7-fold). In contrast, the fractional decrease in oxygen extraction (from normoxia to the lowest oxygen levels tested) was similar at 22 degrees C (1.7-fold) and 30 degrees C (1.5-fold), and clearly smaller than the fractional changes in gill ventilation. In contrast to the almost immediate effects of hypoxia on respiration, bradycardia was not observed until 20 and 30% oxygen saturation at 22 and 30 degrees C, respectively. Bradycardia was, therefore, not observed until below critical oxygen levels. The critical oxygen levels at both temperatures were near or immediately below the accepted 2.3 mg O2 l-1hypoxia threshold for survival, but the increase in the critical oxygen level at 30 degrees C suggests a lower tolerance to hypoxia after an acute increase in temperature. C1 [Capossela, K. M.; Fabrizio, M. C.] Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, Gloucester Point, VA 23062 USA. [Brill, R. W.] Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, James J Howard Marine Sci Lab, Highlands, NJ 07732 USA. [Bushnell, P. G.] Indiana Univ, Dept Biol Sci, South Bend, IN 46634 USA. RP Capossela, KM (reprint author), Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, POB 1346, Gloucester Point, VA 23062 USA. EM kcapossela@dnr.state.md.us OI Fabrizio, Mary/0000-0002-6115-5490 FU Oceanside Conservation Co., Inc. Student Research Grant Program; Eastern Shore Graduate Research Grant FX The authors are grateful to T. Targett for his insight and comments on earlier drafts of the manuscript. The authors also thank the staff of the Virginia Institute of Marine Science Eastern Shore Laboratory for their continuing and genuine hospitality, and for providing access to capture vessels, fish holding and laboratory facilities. This research was supported by funding from the Oceanside Conservation Co., Inc. Student Research Grant Program and the Eastern Shore Graduate Research Grant. This paper is contribution no. 3190 from the Virginia Institute of Marine Science, The College of William & Mary. NR 0 TC 16 Z9 18 U1 0 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD AUG PY 2012 VL 81 IS 3 BP 1043 EP 1058 DI 10.1111/j.1095-8649.2012.03380.x PG 16 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 984UA UT WOS:000307216400010 PM 22880736 ER PT J AU Stocks, HS Verhulst, SA Brown, II Sarkisova, S Casamatta, DA AF Stocks, H. S. Verhulst, S. A. Brown, I. I. Sarkisova, S. Casamatta, D. A. TI LEPTOLYNGBYA FERRUGINOSA SP. NOV., A NOVEL SIDEROPHORIC CYANOBACTERIUM ISOLATED FROM AN IRON-DEPOSITING HOT SPRING SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Stocks, H. S.; Verhulst, S. A.; Casamatta, D. A.] Univ N Florida, Dept Biol Sci, Jacksonville, FL 32224 USA. [Brown, I. I.; Sarkisova, S.] NASA, Johnson Space Ctr, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD AUG PY 2012 VL 48 SU 1 SI SI BP S47 EP S47 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 982NU UT WOS:000307053000134 ER PT J AU Sola, F Xia, ZH Lebron-Colon, M Meador, MA AF Sola, F. Xia, Z. H. Lebron-Colon, M. Meador, M. A. TI Transmission electron microscopy of single wall carbon nanotube/polymer nanocomposites: A first-principles study SO PHYSICA STATUS SOLIDI-RAPID RESEARCH LETTERS LA English DT Article DE transmission electron microscopy; multislice calculations; molecular dynamics simulations; polymer nanocomposites ID POLYMER NANOCOMPOSITES; NANOTUBES; DIFFRACTION AB The physics of high resolution transmission electron microscopy (HRTEM) image formation and electron diffraction of single wall carbon nanotubes (SWCNTs) in a polymer matrix was investigated theoretically on the basis of the multislice method. The effect of the nanocomposite thickness on both image contrast and typical electron diffraction reflections of the nanofillers was explored. The implications of the results on the experimental applicability to study dispersion, chirality and diameter of nanofillers are discussed. (c) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Sola, F.; Lebron-Colon, M.; Meador, M. A.] NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. [Xia, Z. H.] Univ N Texas, Dept Mat Sci & Engn, Denton, TX 76203 USA. RP Sola, F (reprint author), NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. EM francisco.sola-lopez@nasa.gov NR 12 TC 4 Z9 4 U1 0 U2 8 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 1862-6254 EI 1862-6270 J9 PHYS STATUS SOLIDI-R JI Phys. Status Solidi-Rapid Res. Lett. PD AUG PY 2012 VL 6 IS 8 BP 349 EP 351 DI 10.1002/pssr.201206271 PG 3 WC Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Materials Science; Physics GA 994KR UT WOS:000307930100014 ER PT J AU Shelobolina, E Xu, HF Konishi, H Kukkadapu, R Wu, T Blothe, M Roden, E AF Shelobolina, Evgenya Xu, Huifang Konishi, Hiromi Kukkadapu, Ravi Wu, Tao Bloethe, Marco Roden, Eric TI Microbial Lithotrophic Oxidation of Structural Fe(II) in Biotite SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID FERROUS IRON; MOSSBAUER-SPECTROSCOPY; MINERALS; BACTERIA; ROCKS; RHIZOSPHERE; SEDIMENTS; KINETICS; WATER; LIFE AB Microorganisms are known to participate in the weathering of primary phyllosilicate minerals through the production of organic ligands and acids and through the uptake of products of weathering. Here we show that the lithotrophic Fe(II)-oxidizing, nitrate-reducing enrichment culture described by Straub et al. (K.L. Straub, M. Benz, B. Schink, and F. Widdel, Appl. Environ. Microbiol. 62:1458-1460, 1996) can grow via oxidation of structural Fe(II) in biotite, a Fe(II)-rich trioctahedral mica found in granitic rocks. Oxidation of silt/clay-sized biotite particles was detected by a decrease in extractable Fe(II) content and simultaneous nitrate reduction. Mossbauer spectroscopy confirmed structural Fe(II) oxidation. Approximately 1.5 x 10(7) cells were produced per mu mol of Fe(II) oxidized, in agreement with previous estimates of the growth yield of lithoautotrophic circumneutral-pH Fe(II)-oxidizing bacteria. Microbial oxidation of structural Fe(II) resulted in biotite alterations similar to those found in nature, including a decrease in the unit cell b dimension toward dioctahedral levels and Fe and K release. Structural Fe(II) oxidation may involve either direct enzymatic oxidation, followed by solid-state mineral transformation, or indirect oxidation as a result of the formation of aqueous Fe, followed by electron transfer from Fe(II) in the mineral to Fe(III) in solution. Although it is not possible to distinguish between these two mechanisms with available data, the complete absence of aqueous Fe in oxidation experiments favors the former alternative. The demonstration of microbial oxidation of structural Fe(II) suggests that microorganisms are directly responsible for the initial step in the weathering of biotite in granitic aquifers and the plant rhizosphere. C1 [Shelobolina, Evgenya; Xu, Huifang; Konishi, Hiromi; Wu, Tao; Bloethe, Marco; Roden, Eric] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Xu, Huifang; Konishi, Hiromi; Roden, Eric] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI USA. [Kukkadapu, Ravi] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Shelobolina, E (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. EM shelobolina@wisc.edu FU U.S. Department of Energy (DOE), Office of Biological and Environmental Research (BER), Subsurface Biogeochemical Research (SBR) Program [ER64172-1027487-001191]; SBR Scientific Focus Area (SFA) at the Pacific Northwest National Laboratory (PNNL); DOE-BER and located at PNNL, Richland, WA. FX This research was supported by the U.S. Department of Energy (DOE), Office of Biological and Environmental Research (BER), Subsurface Biogeochemical Research (SBR) Program through grant ER64172-1027487-001191 and the SBR Scientific Focus Area (SFA) at the Pacific Northwest National Laboratory (PNNL). Mossbauer spectroscopy measurements were performed at the William Wiley Environmental Molecular Sciences Laboratory (EMSL), a national scientific user facility sponsored by DOE-BER and located at PNNL, Richland, WA. NR 37 TC 22 Z9 22 U1 3 U2 59 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 EI 1098-5336 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD AUG PY 2012 VL 78 IS 16 BP 5746 EP 5752 DI 10.1128/AEM.01034-12 PG 7 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 983SR UT WOS:000307139500033 PM 22685132 ER PT J AU La Duc, MT Vaishampayan, P Nilsson, HR Torok, T Venkateswaran, K AF La Duc, Myron T. Vaishampayan, Parag Nilsson, Henrik R. Torok, Tamas Venkateswaran, Kasthuri TI Pyrosequencing-Derived Bacterial, Archaeal, and Fungal Diversity of Spacecraft Hardware Destined for Mars SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID MICROBIAL DIVERSITY; CLEAN ROOMS; HOSPITAL ENVIRONMENTS; RARE BIOSPHERE; DEEP-SEA; SURVIVAL; RADIATION; IDENTIFICATION; DATABASE; SPORES AB Spacecraft hardware and assembly cleanroom surfaces (233 m(2) in total) were sampled, total genomic DNA was extracted, hypervariable regions of the 16S rRNA gene (bacteria and archaea) and ribosomal internal transcribed spacer (ITS) region (fungi) were subjected to 454 tag-encoded pyrosequencing PCR amplification, and 203,852 resulting high-quality sequences were analyzed. Bioinformatic analyses revealed correlations between operational taxonomic unit (OTU) abundance and certain sample characteristics, such as source (cleanroom floor, ground support equipment [GSE], or spacecraft hardware), cleaning regimen applied, and location about the facility or spacecraft. National Aeronautics and Space Administration (NASA) cleanroom floor and GSE surfaces gave rise to a larger number of diverse bacterial communities (619 OTU; 20 m(2)) than colocated spacecraft hardware (187 OTU; 162 m(2)). In contrast to the results of bacterial pyrosequencing, where at least some sequences were generated from each of the 31 sample sets examined, only 13 and 18 of these sample sets gave rise to archaeal and fungal sequences, respectively. As was the case for bacteria, the abundance of fungal OTU in the GSE surface samples dramatically diminished (9 x less) once cleaning protocols had been applied. The presence of OTU representative of actinobacteria, deinococci, acidobacteria, firmicutes, and proteobacteria on spacecraft surfaces suggests that certain bacterial lineages persist even following rigorous quality control and cleaning practices. The majority of bacterial OTU observed as being recurrent belonged to actinobacteria and alphaproteobacteria, supporting the hypothesis that the measures of cleanliness exerted in spacecraft assembly cleanrooms (SAC) inadvertently select for the organisms which are the most fit to survive long journeys in space. C1 [La Duc, Myron T.; Vaishampayan, Parag; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91125 USA. [Nilsson, Henrik R.] Univ Gothenburg, Dept Biol & Environm Sci, Gothenburg, Sweden. [Torok, Tamas] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Life Sci, Berkeley, CA 94720 USA. RP La Duc, MT (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91125 USA. EM mtladuc@jpl.nasa.gov OI Nilsson, Henrik/0000-0002-8052-0107 NR 62 TC 28 Z9 28 U1 1 U2 38 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD AUG PY 2012 VL 78 IS 16 BP 5912 EP 5922 DI 10.1128/AEM.01435-12 PG 11 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 983SR UT WOS:000307139500054 PM 22729532 ER PT J AU Sprague, AL Sarantos, M Hunten, DM Hill, RE Kozlowski, RWH AF Sprague, A. L. Sarantos, M. Hunten, D. M. Hill, R. E. Kozlowski, R. W. H. TI The lunar sodium atmosphere: April-May 1998 SO CANADIAN JOURNAL OF PHYSICS LA English DT Article ID LEONID METEOR-SHOWER; SOLAR-WIND; EXOSPHERE; MOON; ENHANCEMENT; DESORPTION; POTASSIUM; SURFACE; ORIGIN; TAIL AB Atmospheric sodium at the Moon was observed for altitudes from the ground up to 1800 km from 18 April to 13 May 1998, a period including an entire lunar month. Because of bad weather, coverage was incomplete but we present the analysis of 36 spectra largely from near first and third quarter phases and passage through full moon. The apparatus used was the specially built clear aperture 16.5 cm, 203 cm focal length, Mt. Lemmon Lunar Coronagraph on Mt. Lemmon in the Catalina Mountains of Tucson, Arizona. Data are interpreted in terms of Chamberlain fits to the observed emission rate using both one equivalent temperature and two source components (with both cold and hot density distributions). The extent and equivalent temperatures of the exosphere during this period trended towards an extended coma with very little fraction in the thermally accommodated regime, even near the surface. Preliminary data-model comparisons suggest that these measurements are consistent with rates and spatial distributions expected from a photon-stimulated desorption source, although evidence for one, or possibly two, periods of notable meteoroid impact source might be present. A compilation of new and previously published observations illustrates an increased emission by sodium at third quarter over that of first quarter, a result that suggests that the dayside exospheric content increases, at least occasionally, following transit of the Moon through the Earth's magnetosphere. C1 [Sprague, A. L.; Hunten, D. M.; Hill, R. E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Sarantos, M.] NASA, Heliosphys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sarantos, M.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA. [Kozlowski, R. W. H.] Susquehanna Univ, Dept Phys, Selinsgrove, PA 17890 USA. RP Sprague, AL (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM sprague@lpl.arizona.edu RI Sarantos, Menelaos/H-8136-2013 FU NASA; NSF; NASA Lunar Science Institute via its Dynamic Response of the Environment At the Moon (DREAM) node (NASA) [NNX09AT37A S04] FX We are grateful for the scientific, engineering, and spiritual contributions of our esteemed departed colleagues. Support for this work was provided from 1990 to 1997 by NASA and NSF for DH, RK, AS, and RH. MS was supported from the NASA Lunar Science Institute via its Dynamic Response of the Environment At the Moon (DREAM) node (NASA grant NNX09AT37A S04). In addition, we thank two anonymous reviewers for their helpful and kind reviews. NR 29 TC 5 Z9 5 U1 1 U2 5 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD AUG PY 2012 VL 90 IS 8 BP 725 EP 732 DI 10.1139/p2012-072 PG 8 WC Physics, Multidisciplinary SC Physics GA 993TE UT WOS:000307881700004 ER PT J AU Mattmann, CA Medvidovic, N Malek, S Edwards, G Banerjee, S AF Mattmann, Chris A. Medvidovic, Nenad Malek, Sam Edwards, George Banerjee, Somo TI A Middleware Platform for Providing Mobile and Embedded Computing Instruction to Software Engineering Students SO IEEE TRANSACTIONS ON EDUCATION LA English DT Article DE Glide; mobile computing education; Prism-MW; software architecture; software engineering ID ARCHITECTURAL MIDDLEWARE; SYSTEMS; EXPERIENCE; EDUCATION AB As embedded software systems have grown in number, complexity, and importance in the modern world, a corresponding need to teach computer science students how to effectively engineer such systems has arisen. Embedded software systems, such as those that control cell phones, aircraft, and medical equipment, are subject to requirements and constraints that are significantly different from those encountered in the standard desktop computing environment. For example, embedded systems must frequently address challenges that arise from severe resource restrictions (e.g., low memory and network bandwidth), heterogeneous hardware platforms, and safety-critical operations. Software architecture has been shown to be an effective means for coping with such issues, yet traditional courses on embedded software development rarely focus on software architectural abstractions. Instead, they have concentrated on lower-level issues such as programming languages and hardware interfaces. Since 2005 at the University of Southern California, Los Angeles, a unique course has been developed that affords students the opportunity to gain experience and insights on developing software architectures for embedded systems. At the heart of the course is a middleware platform, Prism-MW, that helps students use software architectural principles to construct embedded systems and understand the important challenges of the embedded systems domain. This paper describes this course through the explanation and evaluation of four years of class projects, weaving together the course, the middleware platform, and the relationship of each to three key pedagogical goals that drove the formulation of the course curriculum. C1 [Mattmann, Chris A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mattmann, Chris A.] Univ So Calif, NASA Jet Prop Lab, Instrument & Sci Data Syst Sect, Los Angeles, CA 90089 USA. [Mattmann, Chris A.; Medvidovic, Nenad] Univ So Calif, Dept Comp Sci, Los Angeles, CA 90089 USA. [Malek, Sam] George Mason Univ, Dept Comp Sci, Volgenau Sch IT & Engn, Fairfax, VA 22030 USA. [Edwards, George] Blue Cell Software, Los Angeles, CA 90069 USA. [Banerjee, Somo] CarsDirect Com, Software Engn, El Segundo, CA 90245 USA. RP Mattmann, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mattmann@jpl.nasa.gov; neno@usc.edu; smalek@gmu.edu; george@bluecellsoftware.com; s.s.banerjee@gmail.com FU National Science Foundation [CCR-9985441, ITR-0312780]; Jet Propulsion Laboratory under National Aeronautics and Space Administration FX This material is based upon work supported by the National Science Foundation under Grants CCR-9985441 and ITR-0312780. The effort was also supported by the Jet Propulsion Laboratory, managed by the California Institute of Technology under a contract from the National Aeronautics and Space Administration. NR 29 TC 1 Z9 1 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9359 EI 1557-9638 J9 IEEE T EDUC JI IEEE Trans. Educ. PD AUG PY 2012 VL 55 IS 3 BP 425 EP 435 DI 10.1109/TE.2012.2182998 PG 11 WC Education, Scientific Disciplines; Engineering, Electrical & Electronic SC Education & Educational Research; Engineering GA 984LO UT WOS:000307191400016 ER PT J AU Glavin, DP Elsila, JE Burton, AS Callahan, MP Dworkin, JP Hilts, RW Herd, CDK AF Glavin, Daniel P. Elsila, Jamie E. Burton, Aaron S. Callahan, Michael P. Dworkin, Jason P. Hilts, Robert W. Herd, Christopher D. K. TI Unusual nonterrestrial L-proteinogenic amino acid excesses in the Tagish Lake meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INTERSTELLAR ICE ANALOGS; CHIRAL-SYMMETRY-BREAKING; MURCHISON METEORITE; CARBONACEOUS CHONDRITES; ASYMMETRIC AUTOCATALYSIS; BIOMOLECULAR CHIRALITY; PARENT BODIES; RACEMIZATION; EVOLUTION; ORIGIN AB The distribution and isotopic and enantiomeric compositions of amino acids found in three distinct fragments of the Tagish Lake C2-type carbonaceous chondrite were investigated via liquid chromatography with fluorescence detection and time-of-flight mass spectrometry and gas chromatography isotope ratio mass spectrometry. Large l-enantiomeric excesses (lee similar to 4359%) of the a-hydrogen aspartic and glutamic amino acids were measured in Tagish Lake, whereas alanine, another a-hydrogen protein amino acid, was found to be nearly racemic (d l) using both techniques. Carbon isotope measurements of d- and l-aspartic acid and d- and l-alanine in Tagish Lake fall well outside of the terrestrial range and indicate that the measured aspartic acid enantioenrichment is indigenous to the meteorite. Alternate explanations for the l-excesses of aspartic acid such as interference from other compounds present in the sample, analytical biases, or terrestrial amino acid contamination were investigated and rejected. These results can be explained by differences in the solidsolution phase behavior of aspartic acid, which can form conglomerate enantiopure solids during crystallization, and alanine, which can only form racemic crystals. Amplification of a small initial l-enantiomer excess during aqueous alteration on the meteorite parent body could have led to the large l-enrichments observed for aspartic acid and other conglomerate amino acids in Tagish Lake. The detection of nonterrestrial l-proteinogenic amino acid excesses in the Tagish Lake meteorite provides support for the hypothesis that significant enantiomeric enrichments for some amino acids could form by abiotic processes prior to the emergence of life. C1 [Glavin, Daniel P.; Elsila, Jamie E.; Callahan, Michael P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burton, Aaron S.] Oak Ridge Associated Univ, NASA, Greenbelt, MD 20771 USA. [Hilts, Robert W.] Grant MacEwan Univ, Dept Phys Sci, Edmonton, AB T5J 4S2, Canada. [Herd, Christopher D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. RP Glavin, DP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM daniel.p.glavin@nasa.gov RI Elsila, Jamie/C-9952-2012; Burton, Aaron/H-2212-2011; Callahan, Michael/D-3630-2012; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Burton, Aaron/0000-0002-7137-1605; Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 FU National Aeronautics and Space Administration (NASA) Astrobiology Institute; Goddard Center for Astrobiology; NASA Cosmochemistry Program; Natural Sciences and Engineering Research Council of Canada; NASA FX Funding support was received from the National Aeronautics and Space Administration (NASA) Astrobiology Institute and the Goddard Center for Astrobiology, the NASA Cosmochemistry Program, and the Natural Sciences and Engineering Research Council of Canada. A. S. Burton is supported by a NASA Postdoctoral Program fellowship administered by Oak Ridge Associated Universities through a contract with NASA. We thank D. N. Simkus for assistance with the meteorite sample preparation and solvent extractions, J. L. Bada for helpful comments on the manuscript, and D. Blackmond and M. Zolensky for valuable discussions. We also appreciate S. Macko, S. Sandford, P. Ehrenfreund, and two anonymous reviewers for careful review of the manuscript. NR 63 TC 41 Z9 42 U1 2 U2 40 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2012 VL 47 IS 8 BP 1347 EP 1364 DI 10.1111/j.1945-5100.2012.01400.x PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 991TB UT WOS:000307723400009 ER PT J AU Oliver, SJ Bock, J Altieri, B Amblard, A Arumugam, V Aussel, H Babbedge, T Beelen, A Bethermin, M Blain, A Boselli, A Bridge, C Brisbin, D Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chania, P Cirasuolo, M Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Dubois, EN Dwek, E Dye, S Eales, S Elbaz, D Farrah, D Feltre, A Ferrero, P Fiolet, N Fox, M Franceschini, A Gear, W Giovannoli, E Glenn, J Gong, Y Solares, EAG Griffin, M Halpern, M Harwit, M Hatziminaoglou, E Heinis, S Hurley, P Hwang, HS Hyde, A Ibar, E Ilbert, O Isaak, K Ivison, RJ Lagache, G Le Floc'h, E Levenson, L Lo Faro, B Lu, N Madden, S Maffei, B Magdis, G Mainetti, G Marchetti, L Marsden, G Marshall, J Mortier, AMJ Nguyen, HT O'Halloran, B Omont, A Page, MJ Panuzzo, P Papageorgiou, A Patel, H Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Raymond, G Rigopoulou, D Riguccini, L Rizzo, D Rodighiero, G Roseboom, IG Rowan-Robinson, M Portal, MS Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Vaccari, M Valtchanov, I Vieira, JD Viero, M Vigroux, L Wang, L Ward, R Wardlow, J Wright, G Xu, CK Zemcov, M AF Oliver, S. J. Bock, J. Altieri, B. Amblard, A. Arumugam, V. Aussel, H. Babbedge, T. Beelen, A. Bethermin, M. Blain, A. Boselli, A. Bridge, C. Brisbin, D. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chania, P. Cirasuolo, M. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Dubois, E. N. Dwek, E. Dye, S. Eales, S. Elbaz, D. Farrah, D. Feltre, A. Ferrero, P. Fiolet, N. Fox, M. Franceschini, A. Gear, W. Giovannoli, E. Glenn, J. Gong, Y. Solares, E. A. Gonzalez Griffin, M. Halpern, M. Harwit, M. Hatziminaoglou, E. Heinis, S. Hurley, P. Hwang, H. S. Hyde, A. Ibar, E. Ilbert, O. Isaak, K. Ivison, R. J. Lagache, G. Le Floc'h, E. Levenson, L. Lo Faro, B. Lu, N. Madden, S. Maffei, B. Magdis, G. Mainetti, G. Marchetti, L. Marsden, G. Marshall, J. Mortier, A. M. J. Nguyen, H. T. O'Halloran, B. Omont, A. Page, M. J. Panuzzo, P. Papageorgiou, A. Patel, H. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Raymond, G. Rigopoulou, D. Riguccini, L. Rizzo, D. Rodighiero, G. Roseboom, I. G. Rowan-Robinson, M. Portal, M. Sanchez Schulz, B. Scott, Douglas Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Vaccari, M. Valtchanov, I. Vieira, J. D. Viero, M. Vigroux, L. Wang, L. Ward, R. Wardlow, J. Wright, G. Xu, C. K. Zemcov, M. TI The Herschel Multi-tiered Extragalactic Survey: HerMES SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE surveys; galaxies: evolution; infrared: galaxies; submillimetre: galaxies ID DEEP-FIELD-SOUTH; STAR-FORMATION HISTORY; LARGE-SCALE STRUCTURE; GOODS-N FIELD; SUBMILLIMETER-SELECTED GALAXIES; 1200-MU-M MAMBO SURVEY; MU-M OBSERVATIONS; SOURCE COUNTS; NUMBER COUNTS; INFRARED GALAXY AB The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling similar to 380?deg2. Fields range in size from 0.01 to similar to 20?deg2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500?mu m) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160?mu m), with an additional wider component of 270?deg2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. The survey will detect of the order of 100?000 galaxies at 5 sigma in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results. C1 [Oliver, S. J.; Dubois, E. N.; Farrah, D.; Hurley, P.; Roseboom, I. G.; Smith, A. J.; Wang, L.; Ward, R.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Bock, J.; Blain, A.; Bridge, C.; Cooray, A.; Dowell, C. D.; Levenson, L.; Lu, N.; Marshall, J.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Vieira, J. D.; Viero, M.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Levenson, L.; Marshall, J.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Altieri, B.; Amblard, A.; Conversi, L.; Portal, M. Sanchez; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Amblard, A.; Arumugam, V.; Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Amblard, A.; Aussel, H.; Elbaz, D.; Hwang, H. S.; Le Floc'h, E.; Magdis, G.; Riguccini, L.] Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Babbedge, T.; Clements, D. L.; Fox, M.; Hyde, A.; Mortier, A. M. J.; O'Halloran, B.; Patel, H.; Rizzo, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Beelen, A.; Bethermin, M.; Fiolet, N.; Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France. [Amblard, A.; Beelen, A.; Bethermin, M.; Fiolet, N.; Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Boselli, A.; Buat, V.; Burgarella, D.; Giovannoli, E.; Heinis, S.; Ilbert, O.] Univ Aix marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Brisbin, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Castro-Rodriguez, N.; Ferrero, P.; Perez-Fournon, I.] IAC, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Castro-Rodriguez, N.; Ferrero, P.; Perez-Fournon, I.] ULL, Dept Astrofis, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. [Cirasuolo, M.; Ibar, E.; Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Cooray, A.; Gong, Y.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dwek, E.] NASA, Observ Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Eales, S.; Gear, W.; Griffin, M.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales. [Feltre, A.; Franceschini, A.; Lo Faro, B.; Mainetti, G.; Marchetti, L.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartmento Astron, I-35122 Padua, Italy. [Fiolet, N.; Omont, A.; Vigroux, L.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Halpern, M.; Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hatziminaoglou, E.] ESO, Garching, Germany. [Isaak, K.] ESTEC SRE SA, ESA Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. [Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Oxford, England. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Chilton, 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. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Oliver, SJ (reprint author), Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. RI Oliver, Seb/A-2479-2013; Magdis, Georgios/C-7295-2014; amblard, alexandre/L-7694-2014; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI Oliver, Seb/0000-0001-7862-1032; Magdis, Georgios/0000-0002-4872-2294; amblard, alexandre/0000-0002-2212-5395; Dye, Simon/0000-0002-1318-8343; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Bethermin, Matthieu/0000-0002-3915-2015; Rodighiero, Giulia/0000-0002-9415-2296; Altieri, Bruno/0000-0003-3936-0284 FU UK Science and Technology Facilities Council [ST/F002858/1, ST/I000976/1]; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX We acknowledge support from the UK Science and Technology Facilities Council, grant numbers ST/F002858/1 and ST/I000976/1. HCSS/HSPOT/HIPE are joint developments by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center and the HIFI, PACS and SPIRE consortia.; SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK) and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). NR 137 TC 264 Z9 263 U1 0 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2012 VL 424 IS 3 BP 1614 EP 1635 DI 10.1111/j.1365-2966.2012.20912.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 982CC UT WOS:000307018300002 ER PT J AU Silvotti, R Ostensen, RH Bloemen, S Telting, JH Heber, U Oreiro, R Reed, MD Farris, LE O'Toole, SJ Lanteri, L Degroote, P Hu, H Baran, AS Hermes, JJ Althaus, LG Marsh, TR Charpinet, S Li, J Morris, RL Sanderfer, DT AF Silvotti, R. Ostensen, R. H. Bloemen, S. Telting, J. H. Heber, U. Oreiro, R. Reed, M. D. Farris, L. E. O'Toole, S. J. Lanteri, L. Degroote, P. Hu, H. Baran, A. S. Hermes, J. J. Althaus, L. G. Marsh, T. R. Charpinet, S. Li, J. Morris, R. L. Sanderfer, D. T. TI Orbital properties of an unusually low-mass sdB star in a close binary system with a white dwarf SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; stars: individual: KIC 6614501; subdwarfs; white dwarfs ID SUBDWARF-B-STARS; PULSAR PSR J1012+5307; COMPACT PULSATORS; NLTT 11748; METALLICITY PROGENITORS; GLOBULAR-CLUSTER; KPD 1930+2752; KEPLER; COMPANION; HELIUM AB We have used 605 days of photometric data from the Kepler spacecraft to study KIC 6614501, a close binary system with an orbital period of 0.157?497?47(25) days (3.779?939 h), that consists of a low-mass subdwarf B (sdB) star and a white dwarf (WD). As seen in many other similar systems, the gravitational field of the WD produces an ellipsoidal deformation of the sdB which appears in the light curve as a modulation at two times the orbital frequency. The ellipsoidal deformation of the sdB implies that the system has a maximum inclination of similar to 40 degrees, with i approximate to 20 degrees being the most likely. The orbital radial velocity (RV) of the sdB star is high enough to produce a Doppler beaming effect with an amplitude of 432 +/- 5 ppm, clearly visible in the folded light curve. The photometric amplitude that we obtain, K1 = 85.8?km?s-1, is similar to 12 per cent less than the spectroscopic RV amplitude of 97.2 +/- 2.0?km?s-1. The discrepancy is due to the photometric contamination from a close object at about 5?arcsec north-west of KIC 6614501, which is difficult to remove. The atmospheric parameters of the sdB star, Teff = 23?700 +/- 500?K and log?g = 5.70 +/- 0.10, imply that it is a rare object below the extreme horizontal branch (EHB), similar to HD 188112. The comparison with different evolutionary tracks suggests a mass between similar to 0.18 and similar to 0.25 M circle dot too low to sustain core helium burning. If the mass was close to 0.180.19 M circle dot, the star could be already on the final He-core WD cooling track. A higher mass, up to similar to 0.25?M circle dot, would be compatible with a He-core WD progenitor undergoing a cooling phase in a H-shell flash loop. A third possibility, with a mass between similar to 0.32 and similar to 0.40 M circle dot, cannot be excluded and would imply that the sdB is a normal (but with an unusually low mass) EHB star burning He in its core. In all these different scenarios, the system is expected to merge in less than 3.1 Gyr due to gravitational wave radiation. C1 [Silvotti, R.; Lanteri, L.] Osservatorio Astrofis Torino, INAF, I-10025 Pino Torinese, Italy. [Ostensen, R. H.; Bloemen, S.; Degroote, P.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Telting, J. H.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Heber, U.] FAU Erlangen Nuremberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Heber, U.] FAU Erlangen Nuremberg, ECAP, Astron Inst, D-96049 Bamberg, Germany. [Oreiro, R.] Inst Astrofis Andalucia, Granada 18008, Spain. [Reed, M. D.; Farris, L. E.; Baran, A. S.] SW Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. [O'Toole, S. J.] Anglo Australian Observ, Epping, NSW 1710, Australia. [Hu, H.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Baran, A. S.] Uniwersytet Pedag, Obserwatorium Suhorze, PL-30084 Krakow, Poland. [Hermes, J. J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Althaus, L. G.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, RA-1900 La Plata, Argentina. [Marsh, T. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Charpinet, S.] Univ Toulouse, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Li, J.; Morris, R. L.; Sanderfer, D. T.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Silvotti, R (reprint author), Osservatorio Astrofis Torino, INAF, Str Osservatorio 20, I-10025 Pino Torinese, Italy. EM silvotti@oato.inaf.it RI Heber, Ulrich/G-3306-2013; OI Heber, Ulrich/0000-0001-7798-6769; Oreiro Rey, Raquel/0000-0002-4899-6199; Silvotti, Roberto/0000-0002-1295-8174; Charpinet, Stephane/0000-0002-6018-6180 FU INAF; European Research Council under European Community [227224]; Research Council of KU Leuven [GOA/2008/04]; Missouri Space Grant; NASA; Netherlands Organization for Scientific Research (NWO); Science and Technology Facilities Council; NASA's Science Mission Directorate FX The authors thank Conny Aerts and Andrew Tkachenko for the work done in organizing and leading the KASC WG9 on binary stars and maintaining its web site, making easier the realization of this paper. They also thank Ronald L. Gilliland, Martin Still and Karen Kinemuchi for useful information on the Kepler pixel data, and the reviewer, Stephan Vennes, for helpful comments on the paper. RS was supported by the PRIN-INAF on 'Asteroseismology: looking inside the stars with space- and ground-based observations'. RHO and SB have received support through the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 227224 (PROSPERITY), as well as from the Research Council of KU Leuven grant agreement GOA/2008/04. MDR and LEF were supported by the Missouri Space Grant, funded by NASA. PD is a Postdoctoral Fellow of the Fund for Scientific Research of Flanders (FWO). HH was supported by the Netherlands Organization for Scientific Research (NWO). TRM was supported by the Science and Technology Facilities Council. Finally, the authors gratefully acknowledge the Kepler team and everybody who has contributed to making this mission possible. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. NR 71 TC 19 Z9 19 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 AUG PY 2012 VL 424 IS 3 BP 1752 EP 1761 DI 10.1111/j.1365-2966.2012.21232.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 982CC UT WOS:000307018300011 ER PT J AU Chini, R Hoffmeister, VH Nasseri, A Stahl, O Zinnecker, H AF Chini, R. Hoffmeister, V. H. Nasseri, A. Stahl, O. Zinnecker, H. TI A spectroscopic survey on the multiplicity of high-mass stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; binaries: general; binaries: spectroscopic; stars: early-type; stars: formation ID ICCD SPECKLE OBSERVATIONS; PRIMORDIAL BINARY POPULATION; YOUNG STELLAR GROUPS; B-TYPE STARS; ECHELLE SPECTROSCOPY; FORMATION MECHANISMS; DISK ACCRETION; RUNAWAY STARS; NEUTRON-STARS; BRIGHT STARS AB The formation of stars above about 20?M circle dot and their apparently high multiplicity remain heavily debated subjects in astrophysics. We have performed a vast high-resolution radial velocity spectroscopic survey of about 250 O- and 540 B-type stars in the southern Milky Way which indicates that the majority of stars (>82?per?cent) with masses above 16?M circle dot form close binary systems while this fraction rapidly drops to 20?per?cent for stars of 3?M circle dot. The binary fractions of O-type stars among different environment classes are: clusters (72 +/- 13?per?cent), associations (73 +/- 8?per?cent), field (43 +/- 13?per?cent) and runaways (69 +/- 11?per?cent). The high frequency of close pairs with components of similar mass argues in favour of a multiplicity originating from the formation process rather than from a tidal capture in a dense cluster. The high binary frequency of runaway O stars that we found in our survey (69?per?cent compared to 1926?per?cent in previous surveys) points to the importance of ejection from young star clusters and thus supports the competitive accretion scenario. C1 [Chini, R.; Hoffmeister, V. H.; Nasseri, A.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Chini, R.] Univ Catolica Norte, Inst Astron, Antofagasta, Chile. [Stahl, O.] Heidelberg Univ, Landessternwarte, ZAH, D-69117 Heidelberg, Germany. [Zinnecker, H.] NASA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Chini, R (reprint author), Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany. EM chini@astro.rub.de FU Nordrhein-Westfalische Akademie der Wissenschaften und der Kunste; state Nordrhein-Westfalen FX We wish to thank K. Fuhrmann, M. Haas, B. Reipurth and B. Stecklum for helpful discussions. This publication is supported as a project of the Nordrhein-Westfalische Akademie der Wissenschaften und der Kunste in the framework of the academy program by the Federal Republic of Germany and the state Nordrhein-Westfalen. NR 49 TC 83 Z9 83 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 AUG PY 2012 VL 424 IS 3 BP 1925 EP 1929 DI 10.1111/j.1365-2966.2012.21317.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 982CC UT WOS:000307018300025 ER PT J AU Huarte-Espinosa, M Frank, A Balick, B Blackman, EG De Marco, O Kastner, JH Sahai, R AF Huarte-Espinosa, M. Frank, A. Balick, B. Blackman, E. G. De Marco, O. Kastner, J. H. Sahai, R. TI From bipolar to elliptical: simulating the morphological evolution of planetary nebulae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; radiative transfer; methods: numerical; stars: AGB and post-AGB; stars: winds, outflows; planetary nebulae: general ID HUBBLE-SPACE-TELESCOPE; POST-AGB STARS; EVOLVED STARS; PROTOPLANETARY NEBULAE; MASS-LOSS; WIND; EMISSION; JETS; PROGENITORS; ENVELOPE AB In this paper we model the evolution of pre-planetary nebula (PPN) and planetary nebula (PN) morphologies as a function of nebular age. The aim of this work is to understand if shape transitions from one evolutionary phase to the other can be driven by changes in the parameters of the mass-loss from the central star. We carry out 2.5D hydrodynamical simulations of mass-loss at the end stages of stellar evolution for intermediate mass stars. Changes in wind velocity, mass-loss rate and mass-loss geometry are tracked. We focus on the transition from mass-loss dominated by a short-duration jet flow (driven during the PPN phase) to mass-loss driven by a spherical fast wind (produced by the central star of the PN). Our results show that while jet-driven nebulae can be expected to be dominated by bipolar morphologies, systems that begin with a jet but are followed by a spherical fast wind will evolve into elliptical objects. Systems that begin with an aspherical asymptotic giant branch wind evolve into butterfly-shaped nebula with, or without, a jet phase. In addition, our models show that spherical nebulae are highly unlikely to derive from either bipolar PPN or elliptical PN over relevant time-scales. The morphological transitions seen in our simulations may however provide insight into the driving mechanisms of both PPN and PN as point to evolutionary changes in the central engine. C1 [Huarte-Espinosa, M.; Frank, A.; Blackman, E. G.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Balick, B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [De Marco, O.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [De Marco, O.] Macquarie Univ, Dept Phys, Sydney, NSW 2109, Australia. [Kastner, J. H.] Rochester Inst Technol, Rochester, NY 14623 USA. [Sahai, R.] NASA JPL, Pasadena, CA USA. RP Huarte-Espinosa, M (reprint author), Univ Rochester, Dept Phys & Astron, 600 Wilson Blvd, Rochester, NY 14627 USA. EM martinhe@pas.rochester.edu FU Space Telescope Science Institute [HST-AR-11251.01-A, HST-AR-12128.01-A]; National Science Foundation [AST-0807363]; Department of Energy [DE-SC0001063]; Cornell University [41843-7012]; Chandra X-ray Observatory Center [GO1-12025A]; NASA [NAS8-03060] FX Financial support for this project was provided by the Space Telescope Science Institute grants HST-AR-11251.01-A and HST-AR-12128.01-A; by the National Science Foundation under award AST-0807363; by the Department of Energy under award DE-SC0001063 and by Cornell University grant 41843-7012. JHK acknowledges financial support by award number GO1-12025A issued to RIT by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. MHE thanks Jonathan Carroll for discussions. We thank the referee Wolfgang Steffen for useful comments that helped to improve this paper. NR 79 TC 17 Z9 17 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2012 VL 424 IS 3 BP 2055 EP 2068 DI 10.1111/j.1365-2966.2012.21348.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 982CC UT WOS:000307018300036 ER PT J AU Meszaros, P Gehrels, N AF Meszaros, Peter Gehrels, Neil TI Gamma-ray bursts and their links with supernovae and cosmology SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS LA English DT Article DE gamma-ray sources; gamma-ray bursts; cosmic rays; neutrinos; supernovae; cosmology; intergalactic medium ID HIGH-ENERGY EMISSION; SHORT GRB 090510; EXTRAGALACTIC BACKGROUND LIGHT; STAR-FORMATION HISTORY; INTERNAL SHOCK MODEL; 28 FEBRUARY 1997; X-RAY; NEUTRON-STAR; FERMI OBSERVATIONS; PROMPT EMISSION AB Gamma-ray bursts are the most luminous explosions in the Universe, whose origin and mechanism are the focus of intense interest. They appear connected to supernova remnants from massive stars or the merger of their remnants, and their brightness makes them temporarily detectable out to the largest distances yet explored in the universe. After pioneering breakthroughs from space and ground experiments, their study is entering a new phase with observations from the recently launched Fermi satellite, as well as the prospect of detections or limits from large neutrino and gravitational wave detectors. The interplay between such observations and theoretical models of gamma-ray bursts is reviewed, as well as their connections to supernovae and cosmology. C1 [Meszaros, Peter] Penn State Univ, Ctr Particle & Gravitat Astrophys, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Meszaros, Peter] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Gehrels, Neil] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Meszaros, P (reprint author), Penn State Univ, Ctr Particle & Gravitat Astrophys, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM nnp@astro.psu.edu; neil.gehrels@nasa.gov FU NASA FX We are grateful to NASA for support, and to our colleagues for many useful discussions. NR 208 TC 13 Z9 13 U1 0 U2 2 PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES PI BEIJING PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA SN 1674-4527 J9 RES ASTRON ASTROPHYS JI Res. Astron. Astrophys. PD AUG PY 2012 VL 12 IS 8 SI SI BP 1139 EP 1161 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 995DB UT WOS:000307987000012 ER PT J AU Self, S Rampino, MR AF Self, Stephen Rampino, Michael R. TI The 1963-1964 eruption of Agung volcano (Bali, Indonesia) SO BULLETIN OF VOLCANOLOGY LA English DT Article DE Agung volcano; Explosive eruption; Plinian deposit; Scoria-and-ash flow deposit; Lava flow; Magma mixing ID TEPHRA-FALL DEPOSITS; STRATOSPHERIC AEROSOLS; VOLUME; THICKNESS; EMISSIONS; DISPERSAL; DYNAMICS; TAMBORA; SULFUR AB The February 1963 to January 1964 eruption of Gunung Agung, Indonesia's largest and most devastating eruption of the twentieth century, was a multi-phase explosive and effusive event that produced both basaltic andesite tephra and andesite lava. A rather unusual eruption sequence with an early lava flow followed by two explosive phases, and the presence of two related but distinctly different magma types, is best explained by successive magma injections and mixing in the conduit or high level magma chamber. The 7.5-km-long blocky-surfaced andesite lava flow of similar to 0.1 km(3) volume was emplaced in the first 26 days of activity beginning on 19 February. On 17 March 1963, a major moderate intensity (similar to 4 x 10(7) kg s(-1)) explosive phase occurred with an similar to 3.5-h-long climax. This phase produced an eruption column estimated to have reached heights of 19 to 26 km above sea level and deposited a scoria lapilli to fine ash fall unit up to similar to 0.2 km(3) (dense rock equivalent-DRE) in volume, with Plinian dispersal characteristics, and small but devastating scoria-and-ash flow deposits. On 16 May, a second intense 4-h-long explosive phase (2.3 x 10(7) kg s(-1)) occurred that produced an similar to 20-km-high eruption column and deposited up to similar to 0.1 km(3) (DRE) volume of similar ash fall and pyroclastic flow deposits, the latter of which were more widespread than in the March phase. The two magma types, porphyritic basaltic andesite and andesite, are found as distinct juvenile scoria populations. This indicates magma mixing prior to the onset of the 1963 eruption, and successive injections of the more mafic magma may have modulated the pulsatory style of the eruption sequence. Even though a total of only similar to 0.4 km(3) (DRE volume) of lava, scoria and ash fall, and scoria-and-ash pyroclastic flow deposits were produced by the 1963 eruption, there was considerable local damage caused mainly by a combination of pyroclastic flows and lahars that formed from the flow deposits in the saturated drainages around Agung. Minor explosive activity and lahar generation by rainfall persisted into early 1964. The climactic events of 17 March and 16 May 1963 managed to inject ash and sulfur-rich gases into the tropical stratosphere. C1 [Rampino, Michael R.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Self, Stephen] Open Univ, Dept Earth & Environm Sci, Milton Keynes MK7 6AA, Bucks, England. [Rampino, Michael R.] NYU, Environm Studies Program, New York, NY 10003 USA. [Rampino, Michael R.] NYU, Dept Biol, New York, NY 10003 USA. RP Rampino, MR (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM mrr1@nyu.edu FU NASA [NSG5145] FX We thank the Indonesian Volcanological Survey, Bandung, West Java, for their hospitality and assistance. K. Kusumadinata provided information and unpublished data; M. Samud and M. Santoso provided assistance in the field. The Indonesian Institute of Science (LIPI) kindly granted permission to work on Bali in 1979. Field work was supported by NASA grant NSG5145. Reviews by J. Fierstein and J. L. Macias, and comments by Associate Editor J. Gardner, considerably improved an earlier version of the manuscript. NR 36 TC 6 Z9 6 U1 2 U2 17 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0258-8900 J9 B VOLCANOL JI Bull. Volcanol. PD AUG PY 2012 VL 74 IS 6 BP 1521 EP 1536 DI 10.1007/s00445-012-0615-z PG 16 WC Geosciences, Multidisciplinary SC Geology GA 976LO UT WOS:000306586400015 ER PT J AU Teverovsky, A AF Teverovsky, Alexander TI Breakdown Voltages in Ceramic Capacitors with Cracks SO IEEE TRANSACTIONS ON DIELECTRICS AND ELECTRICAL INSULATION LA English DT Article DE Electric breakdown; ceramic capacitors; defects; reliability ID DIELECTRIC SURFACE FLASHOVER; CONDUCTION MECHANISM; THIN-FILMS AB Breakdown voltages in 27 types of virgin and fractured X7R multilayer ceramic capacitors (MLCC) rated to voltages from 6.3 to 100 V have been measured and analyzed to evaluate the effectiveness of the dielectric withstanding voltage (DWV) testing to screen-out defective parts and get more insight into breakdown specifics of MLCCs with cracks. Fractures in the parts were introduced mechanically and by thermal shock stress. To simulate exposure of internal electrodes to environments in fractured parts, breakdown testing was carried out also on cross-sectioned and polished capacitors. C1 NASA, Dell Serv Fed Govt Inc, GSFC, Greenbelt, MD 20771 USA. RP Teverovsky, A (reprint author), NASA, Dell Serv Fed Govt Inc, GSFC, Code 562,B 22,Rm C163, Greenbelt, MD 20771 USA. FU NASA Electronic Parts and Packaging (NEPP) program FX This work was sponsored by NASA Electronic Parts and Packaging (NEPP) program. The author is thankful to Michel Sampson, NEPP Program Manager, for support of this investigation, and to Suzanna Douglas (MEI) for assistance with thermal shock testing. NR 28 TC 2 Z9 2 U1 4 U2 21 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1070-9878 J9 IEEE T DIELECT EL IN JI IEEE Trns. Dielectr. Electr. Insul. PD AUG PY 2012 VL 19 IS 4 BP 1448 EP 1455 PG 8 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 987VD UT WOS:000307445000049 ER PT J AU Smith, WL Weisz, E Kireev, SV Zhou, DK Li, ZL Borbas, EE AF Smith, William L., Sr. Weisz, Elisabeth Kireev, Stanislav V. Zhou, Daniel K. Li, Zhenglong Borbas, Eva E. TI Dual-Regression Retrieval Algorithm for Real-Time Processing of Satellite Ultraspectral Radiances SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID SURFACE; EMISSIVITY; PROFILES; CLOUDS AB A fast physically based dual-regression (DR) method is developed to produce, in real time, accurate profile and surface- and cloud-property retrievals from satellite ultraspectral radiances observed for both clear- and cloudy-sky conditions. The DR relies on using empirical orthogonal function (EOF) regression "clear trained" and "cloud trained" retrievals of surface skin temperature, surface-emissivity EOF coefficients, carbon dioxide concentration, cloud-top altitude, effective cloud optical depth, and atmospheric temperature, moisture, and ozone profiles above the cloud and below thin or broken cloud. The cloud-trained retrieval is obtained using cloud-height-classified statistical datasets. The result is a retrieval with an accuracy that is much higher than that associated with the retrieval produced by the unclassified regression method currently used in the International Moderate Resolution Imaging Spectroradiometer/Atmospheric Infrared Sounder (MODIS/AIRS) Processing Package (IMAPP) retrieval system. The improvement results from the fact that the nonlinear dependence of spectral radiance on the atmospheric variables, which is due to cloud altitude and associated atmospheric moisture concentration variations, is minimized as a result of the cloud-height-classification process. The detailed method and results from example applications of the DR retrieval algorithm are presented. The new DR method will be used to retrieve atmospheric profiles from Aqua AIRS, MetOp Infrared Atmospheric Sounding Interferometer, and the forthcoming Joint Polar Satellite System ultraspectral radiance data. C1 [Smith, William L., Sr.; Weisz, Elisabeth; Li, Zhenglong; Borbas, Eva E.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA. [Smith, William L., Sr.; Kireev, Stanislav V.] Hampton Univ, Hampton, VA 23668 USA. [Zhou, Daniel K.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Smith, WL (reprint author), Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, 1225 W Dayton St, Madison, WI 53706 USA. EM bill.l.smith@cox.net RI Li, Zhenglong/A-9375-2013; Weisz, Elisabeth/B-9837-2014; Richards, Amber/K-8203-2015 FU NASA; NOAA FX The development of the DR processing system was made possible through the financial support of NASA and NOAA. The authors are particularly grateful to Drs. Allen Larar, Henry Revercomb, and Allen Huang for their personal interest and encouragement throughout the course of this project. NR 30 TC 19 Z9 19 U1 3 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD AUG PY 2012 VL 51 IS 8 BP 1455 EP 1476 DI 10.1175/JAMC-D-11-0173.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 990DD UT WOS:000307610300002 ER PT J AU Roudebush, JH Orellana, M Bux, S Yi, TH Kauzlarich, SM AF Roudebush, John H. Orellana, Mike Bux, Sabah Yi, Tanghong Kauzlarich, Susan M. TI Crystal structure and thermoelectric properties of clathrate, Ba8Ni3.5Si42.0: Small cage volume and large disorder of the guest atom SO JOURNAL OF SOLID STATE CHEMISTRY LA English DT Article DE Type-I clathrate; Thermoelectrics; Crystal structure; Cation disorder; Vacancies ID THERMAL-CONDUCTIVITY; I CLATHRATE; N-TYPE; SILICON; SUPERSTRUCTURE; BA8-XSI46 AB Samples with the type-I clathrate composition Ba8Ni Si46-x have been synthesized and their structure and thermoelectric properties characterized. Microprobe analysis indicates the Ni incorporation to be 2.62 <= x <= 3.53. The x=3.5 phase crystallizes in the type-I clathrate structure (space group: Pm-3n) with a lattice parameter of 10.2813(3) angstrom. The refined composition was Ba8Ni3.5Si42.0, with small vacancies, 0.4 and 0.5 atoms per formula unit, at the 2a and 6c sites, respectively. The position of the Ba2 atom in the large cage was modeled using a 4-fold split position (24j site): displaced 0.18 angstrom from the cage center (6d site). The volume of the large cage is calculated to be 146 angstrom(3), smaller than other clathrates with similar cation displacement. The sample shows n-type behavior with a maximum of -50 mu V/K at 823 K above which the Seebeck coefficient decreases, suggesting mixed carriers. Lattice thermal conductivity, K-b is 55 mW/K above 600 K. (C) 2012 Elsevier Inc. All rights reserved. C1 [Roudebush, John H.; Orellana, Mike; Yi, Tanghong; Kauzlarich, Susan M.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. [Bux, Sabah] CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, Pasadena, CA 91109 USA. RP Roudebush, JH (reprint author), Univ Calif Davis, Dept Chem, 1 Shields Ave, Davis, CA 95616 USA. EM jhr@princeton.edu RI Yi, Tanghong/F-1866-2011 FU NSF [DMR0600742, DMR 1100313]; National Aeronautics Space Administration FX We gratefully acknowledge the financial support from NSF DMR0600742 and DMR 1100313. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics Space Administration. The authors gratefully acknowledge Dr. Sarah Roeske and Brian Joy for the microprobe analysis and the Jet Propulsion Laboratory (JPL) for the thermoelectric measurements. NR 33 TC 3 Z9 3 U1 1 U2 36 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-4596 J9 J SOLID STATE CHEM JI J. Solid State Chem. PD AUG PY 2012 VL 192 BP 102 EP 108 DI 10.1016/j.jssc.2012.02.054 PG 7 WC Chemistry, Inorganic & Nuclear; Chemistry, Physical SC Chemistry GA 982FM UT WOS:000307028300016 ER PT J AU Baran, AS Reed, MD Stello, D Ostensen, RH Telting, JH Pakstiene, E O'Toole, SJ Silvotti, R Degroote, P Bloemen, S Hu, H Van Grootel, V Clarke, BD Van Cleve, J Thompson, SE Kawaler, SD AF Baran, A. S. Reed, M. D. Stello, D. Ostensen, R. H. Telting, J. H. Pakstiene, E. O'Toole, S. J. Silvotti, R. Degroote, P. Bloemen, S. Hu, H. Van Grootel, V. Clarke, B. D. Van Cleve, J. Thompson, S. E. Kawaler, S. D. TI A pulsation zoo in the hot subdwarf B star KIC 10139564 observed by Kepler SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; techniques: photometric; stars: oscillation; subdwarfs ID COMPACT PULSATORS; DRIVING MECHANISM; MODE; ORIGIN AB We present our analyses of 15?months of Kepler data on KIC?10139564. We detected 57 periodicities with a variety of properties not previously observed all together in one pulsating subdwarf B (sdB) star. Ten of the periodicities were found in the low-frequency region, and we associate them with nonradial g modes. The other periodicities were found in the high-frequency region, which are likely p modes. We discovered that most of the periodicities are components of multiplets with a common spacing. Assuming that multiplets are caused by rotation, we derive a rotation period of 25.6 +/- 1.8?d. The multiplets also allow us to identify the pulsations to an unprecedented extent for this class of pulsator. We also detect l >= 2 multiplets, which are sensitive to the pulsation inclination and can constrain limb darkening via geometric cancellation factors. While most periodicities are stable, we detected several regions that show complex patterns. Detailed analyses showed that these regions are complicated by several factors. Two are combination frequencies that originate in the super-Nyquist region and were found to be reflected below the Nyquist frequency. The Fourier peaks are clear in the super-Nyquist region, but the orbital motion of Kepler smears the Nyquist frequency in the barycentric reference frame and this effect is passed on to the sub-Nyquist reflections. Others are likely multiplets but unstable in amplitudes and/or frequencies. The density of periodicities also makes KIC?10139564 challenging to explain using published models. This menagerie of properties should provide tight constraints on structural models, making this sdB star the most promising for applying asteroseismology. To support our photometric analysis, we have obtained spectroscopic radial-velocity measurements of KIC?10139564 using low-resolution spectra in the Balmer-line region. We did not find any radial-velocity variation. We used our high signal-to-noise average spectrum to improve the atmospheric parameters of the sdB star, deriving Teff?=?31?859?K and log?g?=?5.673?dex. C1 [Baran, A. S.; Reed, M. D.] Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. [Baran, A. S.] Uniwersytet Pedag, Obserwatorium Suhorze, PL-30084 Krakow, Poland. [Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Ostensen, R. H.; Degroote, P.; Bloemen, S.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Telting, J. H.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Pakstiene, E.] Vilnius State Univ, Inst Theoret Phys & Astron, LT-01108 Vilnius, Lithuania. [O'Toole, S. J.] Australian Astron Observ, Epping, NSW 1710, Australia. [Silvotti, R.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Degroote, P.; Bloemen, S.; Hu, H.; Van Grootel, V.; Kawaler, S. D.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Hu, H.] The Observatories, Inst Astron, Cambridge CB3 0HA, England. [Van Grootel, V.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Clarke, B. D.; Van Cleve, J.; Thompson, S. E.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. RP Baran, AS (reprint author), Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. EM sfbaran@cyf-kr.edu.pl OI Silvotti, Roberto/0000-0002-1295-8174 FU Polish Ministry of Science and Higher Education [554/MOB/2009/0]; Missouri Space Grant Consortium; NASA; European Research Council under the European Community's Seventh Framework Programme [227224 (PROSPERITY)]; Research Council of K.U. Leuven [GOA/2008/04]; NASA's Science Mission Directorate FX AB gratefully appreciates funding from the Polish Ministry of Science and Higher Education under project No. 554/MOB/2009/0. MDR was supported by the Missouri Space Grant Consortium, funded by NASA. The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (PROSPERITY), as well as from the Research Council of K.U. Leuven grant agreement GOA/2008/04. PD, SB, HH and SK are grateful for the hospitality during their stay at the Kavli Institute for Theoretical Physics in the framework of the Research Program Asteroseismology in the Space Age. The authors thank U. Heber for kindly providing the spectral model grids. They also thank Tracie Dalton for improving the manuscript by making English correction. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. The authors gratefully acknowledge the Kepler Science Team and all those who have contributed to making the Kepler Mission possible. NR 28 TC 26 Z9 26 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2012 VL 424 IS 4 BP 2686 EP 2700 DI 10.1111/j.1365-2966.2012.21355.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986ZB UT WOS:000307385100022 ER PT J AU Eom, BH Day, PK LeDuc, HG Zmuidzinas, J AF Eom, Byeong Ho Day, Peter K. LeDuc, Henry G. Zmuidzinas, Jonas TI A wideband, low-noise superconducting amplifier with high dynamic range SO NATURE PHYSICS LA English DT Article ID WAVE PARAMETRIC-AMPLIFIER; AMPLIFICATION; ELECTRODYNAMICS; JUNCTIONS; LIMITS AB An ideal amplifier has very low noise, operates over a broad frequency range, and has large dynamic range. Unfortunately, it is difficult to obtain all of these characteristics simultaneously. For example, modern transistor amplifiers offer multi-octave bandwidths and excellent dynamic range, but their noise remains far above the limit set by the uncertainty principle of quantum mechanics. Parametric amplifiers can reach the quantum-mechanical limit, but generally are narrow band and have very limited dynamic range. Here we describe a parametric amplifier that overcomes these limitations through the use of a travelling-wave geometry and the nonlinear kinetic inductance of a superconducting transmission line. We measure gain extending over 2 GHz on either side of an 11.56 GHz pump tone and place an upper limit on the added noise of 3.4 photons at 9.4 GHz. The dynamic range is very large, and the concept can be applied from gigahertz frequencies to similar to 1 THz. C1 [Day, Peter K.; LeDuc, Henry G.; Zmuidzinas, Jonas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eom, Byeong Ho; Zmuidzinas, Jonas] CALTECH, Pasadena, CA 91125 USA. RP Day, PK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Peter.K.Day@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA (Science Mission directorate); Keck Institute for Space Studies; Gordon and Betty Moore Foundation; JPL Research and Technology Development program FX The research was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration and has been supported in part by NASA (Science Mission directorate), the Keck Institute for Space Studies, the Gordon and Betty Moore Foundation and the JPL Research and Technology Development program. NR 35 TC 67 Z9 67 U1 0 U2 30 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 J9 NAT PHYS JI Nat. Phys. PD AUG PY 2012 VL 8 IS 8 BP 623 EP 627 DI 10.1038/NPHYS2356 PG 5 WC Physics, Multidisciplinary SC Physics GA 984WP UT WOS:000307223900015 ER PT J AU Thenkabail, PS Knox, JW Ozdogan, M Gumma, MK Congalton, RG Wu, ZT Milesi, C Finkral, A Marshall, M Mariotto, I You, SC Giri, C Nagler, P AF Thenkabail, Prasad S. Knox, Jerry W. Ozdogan, Mutlu Gumma, Murali Krishna Congalton, Russell G. Wu, Zhuoting Milesi, Cristina Finkral, Alex Marshall, Mike Mariotto, Isabella You, Songcai Giri, Chandra Nagler, Pamela TI ASSESSING FUTURE RISKS TO AGRICULTURAL PRODUCTIVITY, WATER RESOURCES AND FOOD SECURITY: HOW CAN REMOTE SENSING HELP? SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID GLOBAL LAND-COVER; CENTRAL GREAT-PLAINS; TIME-SERIES; IRRIGATED AREAS; MULTITEMPORAL MODIS; CROP PRODUCTION; CLIMATE-CHANGE; CROPLANDS; DATABASE; AVHRR C1 [Knox, Jerry W.] Cranfield Univ, Cranfield Water Sci Inst, Bedford, England. [Ozdogan, Mutlu] Univ Wisconsin, Madison, WI 53706 USA. [Congalton, Russell G.] Univ New Hampshire, Durham, NH 03824 USA. [Wu, Zhuoting] No Arizona Univ, Flagstaff, AZ 86011 USA. [Milesi, Cristina] California State Univ Monterey Bay, NASA, Monterey, CA USA. [Mariotto, Isabella] Univ Arizona, Tucson, AZ 85721 USA. EM pthenkabail@usgs.gov RI Knox, Jerry/A-4793-2010; OI Knox, Jerry/0000-0002-0473-6440; Ozdogan, Mutlu/0000-0002-1707-3375 FU U. S. Geological Survey's (USGS) John Wesley Powell Center for Analysis and Synthesis; USGS Geographic Analysis and Monitoring (GAM); Land Remote Sensing (LRS) programs FX Authors would like to thank U. S. Geological Survey's (USGS) John Wesley Powell Center for Analysis and Synthesis (http://powellcenter.usgs.gov/) for funding the Working Group on Global Croplands (WGGC) :http://powellcenter.usgs.gov/current_projects. php#GlobalCroplandsAbstract. Our special thanks to Powell Center Directors: Dr. Jill Baron and Dr. Marty Goldhaber for guidance and in-sights. Review comments from Dr. Laura Norman, Dr. Cynthia Wallace, and Dr. Dennis Dye of USGS are acknowledged. Funding support from USGS Geographic Analysis and Monitoring (GAM) and Land Remote Sensing (LRS) programs are gratefully acknowledged. Support of the Western Geographic Science Center leadership, in particular Mr. Edwin Pfeifer and Dr. Susan P Benjamin is deeply appreciated. Logistical support for the working group activities provided by Ms. Lone Hughes is gratefully acknowledged. Computing support from Mr. Tim Kern and his team (Ms. Megan Eberhardt Frank, Mr. Thomas W. Miller, Ms. Gail A. Montgomery and others) is much appreciated. NR 42 TC 25 Z9 26 U1 0 U2 28 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 AUG PY 2012 VL 78 IS 8 SI SI BP 773 EP 782 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 982ZE UT WOS:000307084900001 ER PT J AU Blackmore, L Acikmese, B Carson, JM AF Blackmore, Lars Acikmese, Behcet Carson, John M., III TI Lossless convexification of control constraints for a class of nonlinear optimal control problems SO SYSTEMS & CONTROL LETTERS LA English DT Article DE Optimal control theory; Control of constrained systems; Guidance, navigation and control of vehicles ID POWERED-DESCENT GUIDANCE; IMAGE SEGMENTATION; OPTIMIZATION AB In this paper we consider a class of optimal control problems that have continuous-time nonlinear dynamics and nonconvex control constraints. We propose a convex relaxation of the nonconvex control constraints, and prove that the optimal solution to the relaxed problem is the globally optimal solution to the original problem with nonconvex control constraints. This lossless convexification enables a computationally simpler problem to be solved instead of the original problem. We demonstrate the approach in simulation with a planetary soft landing problem involving a nonlinear gravity field. (C) 2012 Elsevier B.V. All rights reserved. C1 [Blackmore, Lars] Space Explorat Technol, Hawthorne, CA 90250 USA. [Acikmese, Behcet; Carson, John M., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Blackmore, L (reprint author), Space Explorat Technol, 1 Rocket Rd, Hawthorne, CA 90250 USA. EM larsb@mit.edu; behcet@jpl.nasa.gov; jmcarson@jpl.nasa.gov FU National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration.(C)2011 California Institute of Technology. Government sponsorship acknowledged. NR 38 TC 9 Z9 10 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-6911 J9 SYST CONTROL LETT JI Syst. Control Lett. PD AUG PY 2012 VL 61 IS 8 BP 863 EP 870 DI 10.1016/j.sysconle.2012.04.010 PG 8 WC Automation & Control Systems; Operations Research & Management Science SC Automation & Control Systems; Operations Research & Management Science GA 991JO UT WOS:000307697500007 ER PT J AU McGrath-Spangler, EL Denning, AS AF McGrath-Spangler, Erica L. Denning, A. Scott TI Estimates of North American summertime planetary boundary layer depths derived from space-borne lidar SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERE INTERACTIONS; SOUTHEAST PACIFIC; AIRBORNE LIDAR; BOREAL FOREST; MIXING HEIGHT; ENTRAINMENT AB The planetary boundary layer (PBL) mediates exchanges of energy, moisture, momentum, carbon, and pollutants between the surface and the atmosphere. This paper is a first step in producing a space-based estimate of PBL depth that can be used to compare with and evaluate model-based PBL depth retrievals, inform boundary layer studies, and improve understanding of the above processes. In clear sky conditions, space-borne lidar backscatter is frequently affected by atmospheric properties near the PBL top. Spatial patterns of 5-year mean mid-day summertime PBL depths over North America were estimated from the CALIPSO lidar backscatter and are generally consistent with model reanalyses and AMDAR (Aircraft Meteorological DAta Reporting) estimates. The rate of retrieval is greatest over the subtropical oceans (near 100%) where overlying subsidence limits optically thick clouds from growing and attenuating the lidar signal. The general retrieval rate over land is around 50% with decreased rates over the Southwestern United States and regions with high rates of convection. The lidar-based estimates of PBL depth tend to be shallower than aircraft estimates in coastal areas. Compared to reanalysis products, lidar PBL depths are greater over the oceans and areas of the boreal forest and shallower over the arid and semiarid regions of North America. C1 [McGrath-Spangler, Erica L.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [McGrath-Spangler, Erica L.; Denning, A. Scott] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP McGrath-Spangler, EL (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM emcgrath@atmos.colostate.edu RI McGrath-Spangler, Erica/H-1985-2012; Denning, Scott/F-4974-2011; OI Denning, Scott/0000-0003-3032-7875; McGrath-Spangler, Erica/0000-0002-8540-5423 FU National Science Foundation (NSF); National Aeronautics and Space Administration grant [NNX08AV04H] FX The NARR data for this study are from the Research Data Archive (RDA), which is maintained by the Computational and Information Systems Laboratory (CISL) at the National Center for Atmospheric Research (NCAR). NCAR is sponsored by the National Science Foundation (NSF). The MERRA data for this study are from the Global Modeling and Assimilation Office (GMAO) and the Goddard Earth Sciences Data and Information Services Center (GES DISC). The original data are available from the RDA (http://dss.ucar.edu) in data set number ds608.0. This study was made possible in part due to the data made available to the National Oceanic and Atmospheric Administration by the following commercial airlines: American, Delta, Federal Express, Northwest, Southwest, United, and United Parcel Service. We would like to thank Nikisa Jordan and Mark Vaughan for their assistance with the CALIPSO data and the PBL depth algorithm. We would also like to thank David Randall for many helpful suggestions that improved this manuscript substantially. This research was supported by National Aeronautics and Space Administration grant NNX08AV04H. NR 31 TC 14 Z9 15 U1 3 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 1 PY 2012 VL 117 AR D15101 DI 10.1029/012JD017615 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 988EM UT WOS:000307471400002 ER PT J AU Iguchi, T Nakajima, T Khain, AP Sait, K Takemura, T Okamoto, H Nishizawa, T Tao, WK AF Iguchi, Takamichi Nakajima, Teruyuki Khain, Alexander P. Sait, Kazuo Takemura, Toshihiko Okamoto, Hajime Nishizawa, Tomoaki Tao, Wei-Kuo TI Evaluation of Cloud Microphysics in JMA-NHM Simulations Using Bin or Bulk Microphysical Schemes through Comparison with Cloud Radar Observations SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID MESOSCALE MODEL; PROFILING RADAR; RESOLVING MODEL; DOPPLER RADAR; SATELLITE; ICE; PRECIPITATION; RETRIEVAL; PACKAGE AB Numerical weather prediction (NWP) simulations using the Japan Meteorological Agency Nonhydrostatic Model (JMA-NHM) are conducted for three precipitation events observed by shipborne or spaceborne W-band cloud radars. Spectral bin and single-moment bulk cloud microphysics schemes are employed separately for an intercomparative study. A radar product simulator that is compatible with both microphysics schemes is developed to enable a direct comparison between simulation and observation with respect to the equivalent radar reflectivity factor Ze, Doppler velocity (DV), and path-integrated attenuation (PIA). In general, the bin model simulation shows better agreement with the observed data than the bulk model simulation. The correction of the terminal fall velocities of snowflakes using those of hail further improves the result of the bin model simulation. The results indicate that there are substantial uncertainties in the mass-size and size-terminal fall velocity relations of snowflakes or in the calculation of terminal fall velocity of snow aloft. For the bulk microphysics, the overestimation of Ze is observed as a result of a significant predominance of snow over cloud ice due to substantial deposition growth directly to snow. The DV comparison shows that a correction for the fall velocity of hydrometeors considering a change of particle size should be introduced even in single-moment bulk cloud microphysics. C1 [Iguchi, Takamichi; Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Iguchi, Takamichi] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Nakajima, Teruyuki] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba, Japan. [Khain, Alexander P.] Hebrew Univ Jerusalem, Inst Life Sci, Dept Atmospher Sci, IL-91904 Jerusalem, Israel. [Sait, Kazuo] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan. [Takemura, Toshihiko; Okamoto, Hajime] Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan. [Nishizawa, Tomoaki] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. RP Iguchi, T (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. EM takamichi.iguchi@nasa.gov RI Takemura, Toshihiko/C-2822-2009; Okamoto, Hajime/E-6510-2010; Nakajima, Teruyuki/H-2370-2013; Kyushu, RIAM/F-4018-2015; U-ID, Kyushu/C-5291-2016; Measurement, Global/C-4698-2015 OI Takemura, Toshihiko/0000-0002-2859-6067; Okamoto, Hajime/0000-0002-4540-1698; Nakajima, Teruyuki/0000-0002-9042-504X; FU JAXA/EarthCARE; JAXA/GCOM; MEXT/VL for Climate System Diagnostics; MOE/Global Environment Research Fund [A-1101]; NIES/GOSAT; JST/CREST; MEXT/RECCA/SALSA; Israel Science Foundation [140/07]; NASA Precipitation Measuring Mission (PMM); NASA Modeling, Analysis, and Prediction (MAP) Program; Toshiro Inoue of the Atmospheric and Ocean Research Institute; Yuichiro Hagihara of the Research Institute for Applied Mechanics FX This study was supported by the projects, JAXA/EarthCARE, JAXA/GCOM, MEXT/VL for Climate System Diagnostics, MOE/Global Environment Research Fund A-1101, NIES/GOSAT, JST/CREST, and MEXT/RECCA/SALSA. One of the authors (A. Khain) is supported by a grant from the Israel Science Foundation (140/07). Another author (Tao) is supported by the NASA Precipitation Measuring Mission (PMM) and the NASA Modeling, Analysis, and Prediction (MAP) Program. The authors wish to acknowledge the developers of the JMA-NHM and HUCM. We also thank the persons associated with JAMSTEC for conducting the observation mission on the Research Vessel Mirai and Hiroshi Kumagai of the National Institute of Information and Communications Technology for development of the shipborne radar. Cloud Sat products were provided by the Cloud Sat Data Processing Center with the NASA Cloud Sat project; the processing was supported by Toshiro Inoue of the Atmospheric and Ocean Research Institute and Yuichiro Hagihara of the Research Institute for Applied Mechanics. Stephen Palm of the Science Systems and Applications, Inc., is also thanked for valuable discussion on improving the manuscript. NR 51 TC 3 Z9 3 U1 3 U2 16 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD AUG PY 2012 VL 69 IS 8 BP 2566 EP 2586 DI 10.1175/JAS-D-11-0213.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 983XB UT WOS:000307150900015 ER PT J AU Boy, JP Hinderer, J de Linage, C AF Boy, Jean-Paul Hinderer, Jacques de Linage, Caroline TI Retrieval of Large-Scale Hydrological Signals in Africa from GRACE Time-Variable Gravity Fields SO PURE AND APPLIED GEOPHYSICS LA English DT Article DE Time-variable gravity; global change from geodesy; hydrology; Africa ID WATER STORAGE; PRECIPITATION; BASIN; MODELS; ASSIMILATION; INVERSION; SYSTEM; AMAZON AB Since its launch in April 2002, the Gravity Recovery and Climate Experiment (GRACE) mission is recording the Earth's time-variable gravity field with temporal and spatial resolutions of typically 7-30 days and a few hundreds of kilometers, allowing the monitoring of continental water storage variations from both continental and river-basin scales. We investigate here large scale hydrological variations in Africa using different GRACE spherical harmonic solutions, using different processing strategies (constrained and unconstrained solutions). We compare our GRACE estimates to different global hydrology models, with different land-surface schemes and also precipitation forcing. We validate GRACE observations through two different techniques: first by studying desert areas, providing an estimate of the precision. Then we compare GRACE recovered mass variations of main lakes to volume changes derived from radar altimetry measurements. We also study the differences between different publicly available precipitation datasets from both space measurements and ground rain gauges, and their impact on soil-moisture estimates. C1 [Boy, Jean-Paul; Hinderer, Jacques] EOST IPGS UMR 7516 CNRS UdS, F-67084 Strasbourg, France. [Boy, Jean-Paul] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [de Linage, Caroline] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. RP Boy, JP (reprint author), EOST IPGS UMR 7516 CNRS UdS, 5 Rue Rene Descartes, F-67084 Strasbourg, France. EM jeanpaul.boy@unistra.fr; jacques.hinderer@unistra.fr; caroline.delinage@uci.edu RI Boy, Jean-Paul/E-6677-2017 OI Boy, Jean-Paul/0000-0003-0259-209X FU Marie Curie International Outgoing Fellowship [PIOF-GA-2008-221753]; French Agence Nationale de la Recherche (ANR) (GHYRAF project); Centre National d'Etudes Spatiale (CNES) grant FX Jean-Paul Boy was visiting NASA Goddard Space Flight Center, with a Marie Curie International Outgoing Fellowship (No. PIOF-GA-2008-221753). This project is partly funded by the French Agence Nationale de la Recherche (ANR) (GHYRAF project) and partly by a Centre National d'Etudes Spatiale (CNES) grant. The GLDAS data used in this study were acquired as part of the mission of NASA's Earth Science Division and archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC). We thank B. F. Chao and an anonymous reviewer for their comments that helped improving the manuscript. NR 40 TC 3 Z9 3 U1 2 U2 20 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD AUG PY 2012 VL 169 IS 8 BP 1373 EP 1390 DI 10.1007/s00024-011-0416-x PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 975YH UT WOS:000306547200005 ER PT J AU Hinderer, J Pfeffer, J Boucher, M Nahmani, S De Linage, C Boy, JP Genthon, P Seguis, L Favreau, G Bock, O Descloitres, M AF Hinderer, J. Pfeffer, J. Boucher, M. Nahmani, S. De Linage, C. Boy, J-P. Genthon, P. Seguis, L. Favreau, G. Bock, O. Descloitres, M. CA GHYRAF Team TI Land Water Storage Changes from Ground and Space Geodesy: First Results from the GHYRAF (Gravity and Hydrology in Africa) Experiment SO PURE AND APPLIED GEOPHYSICS LA English DT Article DE African monsoon; Sahel; water storage; gravimetry; GPS; MRS; GRACE ID GLOBAL GEODYNAMICS PROJECT; TIME-VARIABLE GRAVITY; SUPERCONDUCTING GRAVIMETER; MAGNETIC-RESONANCE; GRACE; FIELD; PRECIPITATION; AQUIFER; SYSTEM; NIGER AB This paper is devoted to the first results from the GHYRAF (Gravity and Hydrology in Africa) experiment conducted since 2008 in West Africa and is aimed at investigating the changes in water storage in different regions sampling a strong rainfall gradient from the Sahara to the monsoon zone. The analysis of GPS vertical displacement in Niamey (Niger) and Djougou (Benin) shows that there is a clear annual signature of the hydrological load in agreement with global hydrology models like GLDAS. The comparison of GRACE solutions in West Africa, and more specifically in the Niger and Lake Chad basins, reveals a good agreement for the large scale annual water storage changes between global hydrology models and space gravity observations. Ground gravity observations done with an FG5 absolute gravimeter also show signals which can be well related to measured changes in soil and ground water. We present the first results for two sites in the Sahelian band (Wankama and Diffa in Niger) and one (Djougou in Benin) in the Sudanian monsoon region related to the recharge-discharge processes due to the monsoonal event in summer 2008 and the following dry season. It is confirmed that ground gravimetry is a useful tool to constrain local water storage changes when associated to hydrological and subsurface geophysical in situ measurements. C1 [Hinderer, J.; Pfeffer, J.; Boy, J-P.] Univ Strasbourg, Inst Phys Globe Strasbourg, UMR CNRS 7516, F-67084 Strasbourg, France. [Boucher, M.; Genthon, P.; Seguis, L.; Favreau, G.] Univ Montpellier 2, IRD, UMR CNRS 5569, F-34095 Montpellier, France. [De Linage, C.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Nahmani, S.; Bock, O.] LAREG IGN, F-77455 Marne La Vallee, France. [Boy, J-P.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Boucher, M.; Descloitres, M.] Univ Grenoble 1, Lab Etud Transferts Hydrol & Environm, UMR CNRS 5564, INPG,IRD, F-38041 Grenoble, France. RP Hinderer, J (reprint author), Univ Strasbourg, Inst Phys Globe Strasbourg, UMR CNRS 7516, F-67084 Strasbourg, France. EM Jacques.Hinderer@eost.u-strasbg.fr RI Favreau, guillaume/A-7573-2008; Boucher, Marie/M-7393-2016; Boy, Jean-Paul/E-6677-2017 OI Favreau, guillaume/0000-0001-7358-9301; Boucher, Marie/0000-0003-4994-2448; Boy, Jean-Paul/0000-0003-0259-209X FU French Agence Nationale de la Recherche (ANR); INSU-CNRS FX This project is funded by the French Agence Nationale de la Recherche (ANR) for 4 years (2008-2011). The strong logistic and manpower support found in Niger and Benin is available thanks to the Institut de Recherche pour le Developpement (IRD). Assistance of local water authorities in Niger and Benin is also warmly acknowledged. We also acknowledge the support of INSU-CNRS to run the AMMA-CATCH observatory in West Africa (http://www.amma-catch.org). NR 62 TC 12 Z9 12 U1 4 U2 39 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD AUG PY 2012 VL 169 IS 8 BP 1391 EP 1410 DI 10.1007/s00024-011-0417-9 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 975YH UT WOS:000306547200006 ER PT J AU Boxe, CS Hamer, PD Ford, W Hoffmann, M Shallcross, DE AF Boxe, C. S. Hamer, P. D. Ford, W. Hoffmann, M. Shallcross, D. E. TI The effect of the novel HO2+NO -> HNO3 reaction channel at South Pole, Antarctica SO ANTARCTIC SCIENCE LA English DT Article DE boundary layer; ice photochemistry; nitric acid; NOx; ozone; polar chemistry ID BOUNDARY-LAYER; ISCAT 2000; NITRATE PHOTOCHEMISTRY; ATMOSPHERIC CHEMISTRY; NOX EMISSIONS; SNOW; IMPACT; HOX; HO2+NOREACTION; REASSESSMENT AB It is well established that the reaction of HO2 with NO plays a central role in atmospheric chemistry, by way of OH/HO2 recycling and reduction of ozone depletion by HOx cycles in the stratosphere and through ozone production in the troposphere. Utilizing a photochemical box model, we investigate the impact of the recently observed HNO3 production channel (HO2 + NO -> HNO3) on NOx (NO + NO2), HOx (OH + HO2), HNO3, and O-3 concentrations in the boundary layer at the South Pole, Antarctica. Our simulations exemplify decreases in peak O-3, NO, NO2, and OH and an increase in HNO3. Also, mean OH is in better agreement with observations, while worsening the agreement with O-3, HO2, and HNO3 concentrations observed at the South Pole. The reduced concentrations of NOx are consistent with expected decreases in atmospheric NOx lifetime as a result of increased sequestration of NOx into HNO3. Although we show that the inclusion of the novel HNO3 production channel brings better agreement of OH with field measurements, the modelled ozone and HNO3 are worsened, and the changes in NOx lifetime imply that snowpack NOx emissions and snowpack nitrate recycling must be re-evaluated. C1 [Boxe, C. S.; Hamer, P. D.] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. [Ford, W.; Hoffmann, M.] CALTECH, Pasadena, CA 91125 USA. [Shallcross, D. E.] Univ Bristol, Sch Chem, Bristol BS8 1TS, Avon, England. RP Boxe, CS (reprint author), CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. EM boxeman3@gmail.com RI Chem, GEOS/C-5595-2014 FU National Aeronautics and Space Administration (NASA) FX Paul Hamer 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 the National Aeronautics and Space Administration (NASA). The work described here was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contracts with NASA. The constructive comments of the reviewers are gratefully acknowledged. NR 39 TC 1 Z9 1 U1 1 U2 20 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0954-1020 EI 1365-2079 J9 ANTARCT SCI JI Antarct. Sci. PD AUG PY 2012 VL 24 IS 4 BP 417 EP 425 DI 10.1017/S0954102012000144 PG 9 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 983TM UT WOS:000307141600011 ER PT J AU James, JT Zalesak, SM AF James, John T. Zalesak, Selina M. TI Prediction of Crew Health Effects from Air Samples Taken Aboard the International Space Station SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE mixtures; air pollution; spaceflight; inhalation toxicity; occupational health ID RATS; ACETALDEHYDE; FORMALDEHYDE; ACROLEIN; MIXTURES AB JAMES JT, ZALESAK SM. Prediction of crew health effects from air samples taken aboard the International Space Station. Aviat Space Environ Med 2012; 83:795-9. Introduction: Spaceflight aboard the International Space Station (ISS) involves stays of individual crewmembers for up to 6 mo during which they are exposed to a complex mixture of airborne pollutants. Methods to predict specific health effects from exposure to a mixture of air pollutants are not well developed. Herein, air monitoring data from the ISS are used to demonstrate a new method to estimate a threshold for possible health effects from exposure to mixtures. Methods: An empirical, additive approach was developed to transform monthly air pollutant data, which had been obtained primarily by gas chromatography-mass spectrometry from samples of ISS air, to threshold (T) values for 16 adverse health effect groups. Spacecraft maximum allowable concentrations (SMACs), available for most spacecraft air pollutants, were used to form target-organ/effect groups, from which group T values were estimated. If T > 1 for a group, then there is an unacceptable risk of the toxic effect. Results: Samples of air taken from the ISS in 2010 revealed that all 16 toxicological groups were within safe limits. Highest T values were as follows: mucosal irritants (0.53 +/- 0.44), headache (0.52 +/- 0.06), central nervous system depression (0.25 +/- 0.06), and cardiac sensitization (0.13 +/- 0.04). Discussion: The additive model is supported by limited inhalation data on rats in the literature. Our predictions of no adverse effect on crew health are useful as part of NASA's Lifetime Surveillance of Astronaut Health (LSAH). If one of the 16 levels had exceeded T = 1, then standard surveillance could be supplemented to address this potential health risk. C1 [James, John T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP James, JT (reprint author), 2101 NASA Pkwy,SF2, Houston, TX 77058 USA. EM john.t.james@nasa.gov NR 11 TC 0 Z9 0 U1 3 U2 11 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD AUG PY 2012 VL 83 IS 8 BP 795 EP 799 DI 10.3357/ASEM.3237.2012 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 981AC UT WOS:000306936600010 PM 22872995 ER PT J AU Jiang, XN Waliser, DE Kim, D Zhao, M Sperber, KR Stern, WF Schubert, SD Zhang, GJ Wang, WQ Khairoutdinov, M Neale, RB Lee, MI AF Jiang, Xianan Waliser, Duane E. Kim, Daehyun Zhao, Ming Sperber, Kenneth R. Stern, William F. Schubert, Siegfried D. Zhang, Guang J. Wang, Wanqiu Khairoutdinov, Marat Neale, Richard B. Lee, Myong-In TI Simulation of the intraseasonal variability over the Eastern Pacific ITCZ in climate models SO CLIMATE DYNAMICS LA English DT Article DE Intraseasonal variability; Eastern Pacific warm pool; ITCZ ID MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODELS; NORTH-AMERICAN-MONSOON; WEST-AFRICAN MONSOON; COUPLED EQUATORIAL WAVES; CLOUD-RESOLVING MODEL; FORECAST SYSTEM MODEL; LARGE-SCALE MODELS; GULF-OF-MEXICO; BOREAL SUMMER AB During boreal summer, convective activity over the eastern Pacific (EPAC) inter-tropical convergence zone (ITCZ) exhibits vigorous intraseasonal variability (ISV). Previous observational studies identified two dominant ISV modes over the EPAC, i.e., a 40-day mode and a quasi-biweekly mode (QBM). The 40-day ISV mode is generally considered a local expression of the Madden-Julian Oscillation. However, in addition to the eastward propagation, northward propagation of the 40-day mode is also evident. The QBM mode bears a smaller spatial scale than the 40-day mode, and is largely characterized by northward propagation. While the ISV over the EPAC exerts significant influences on regional climate/weather systems, investigation of contemporary model capabilities in representing these ISV modes over the EPAC is limited. In this study, the model fidelity in representing these two dominant ISV modes over the EPAC is assessed by analyzing six atmospheric and three coupled general circulation models (GCMs), including one super-parameterized GCM (SPCAM) and one recently developed high-resolution GCM (GFDL HIRAM) with horizontal resolution of about 50 km. While it remains challenging for GCMs to faithfully represent these two ISV modes including their amplitude, evolution patterns, and periodicities, encouraging simulations are also noted. In general, SPCAM and HIRAM exhibit relatively superior skill in representing the two ISV modes over the EPAC. While the advantage of SPCAM is achieved through explicit representation of the cumulus process by the embedded 2-D cloud resolving models, the improved representation in HIRAM could be ascribed to the employment of a strongly entraining plume cumulus scheme, which inhibits the deep convection, and thus effectively enhances the stratiform rainfall. The sensitivity tests based on HIRAM also suggest that fine horizontal resolution could also be conducive to realistically capture the ISV over the EPAC, particularly for the QBM mode. Further analysis illustrates that the observed 40-day ISV mode over the EPAC is closely linked to the eastward propagating ISV signals from the Indian Ocean/Western Pacific, which is in agreement with the general impression that the 40-day ISV mode over the EPAC could be a local expression of the global Madden-Julian Oscillation (MJO). In contrast, the convective signals associated with the 40-day mode over the EPAC in most of the GCM simulations tend to originate between 150A degrees E and 150A degrees W, suggesting the 40-day ISV mode over the EPAC might be sustained without the forcing by the eastward propagating MJO. Further investigation is warranted towards improved understanding of the origin of the ISV over the EPAC. C1 [Jiang, Xianan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jiang, Xianan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Kim, Daehyun] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA. [Zhao, Ming; Stern, William F.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Sperber, Kenneth R.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Wang, Wanqiu] NOAA, Natl Ctr Environm Predict, Camp Springs, MD USA. [Khairoutdinov, Marat] SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA. [Neale, Richard B.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Lee, Myong-In] Ulsan Natl Inst Sci & Technol, Seoul, South Korea. RP Jiang, XN (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM xianan@jifresse.ucla.edu RI Jiang, Xianan/A-2283-2012; Zhao, Ming/C-6928-2014; Sperber, Kenneth/H-2333-2012; OI Lee, Myong-In/0000-0001-8983-8624 FU NOAA CPPA program [NA09OAR4310191]; NSF Climate and Large-Scale Dynamics [ATM-0934285]; US Department of Energy Office of Science, Regional and Global Climate Modeling Program by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; NASA [NNX09AK34G]; National Aeronautics and Space Administration FX We thank anonymous reviewers for their critical comments on an earlier version of this manuscript. Thanks also to Terry Kubar for his comments and editorial assistance. The first author (XJ) acknowledges support by NOAA CPPA program under Award NA09OAR4310191 and NSF Climate and Large-Scale Dynamics under Award ATM-0934285. K. Sperber was supported under the auspices of the US Department of Energy Office of Science, Regional and Global Climate Modeling Program by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. DK was supported by NASA grant NNX09AK34G. We thank U.S. CLIVAR MJO Working Group for coordinating this model comparison activity and modeling centers for providing the model output. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 84 TC 9 Z9 9 U1 0 U2 21 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD AUG PY 2012 VL 39 IS 3-4 BP 617 EP 636 DI 10.1007/s00382-011-1098-x PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 985MQ UT WOS:000307271200006 ER PT J AU Di Biagio, C di Sarra, A Eriksen, P Ascanius, SE Muscari, G Holben, B AF Di Biagio, C. di Sarra, A. Eriksen, P. Ascanius, S. E. Muscari, G. Holben, B. TI Effect of surface albedo, water vapour, and atmospheric aerosols on the cloud-free shortwave radiative budget in the Arctic SO CLIMATE DYNAMICS LA English DT Article DE Arctic radiative balance; Surface albedo; Atmospheric aerosols; Water vapour; Direct radiative forcing; Arctic amplification ID OPTICAL-PROPERTIES; SEA-ICE; TRENDS; ALGORITHM; POLLUTION; AERONET; EVENTS; SHEBA; MODIS AB This study is based on ground-based measurements of downward surface shortwave irradiance (SW), columnar water vapour (wv), and aerosol optical depth (tau) obtained at Thule Air Base (Greenland) in 2007-2010, together with MODIS observations of the surface shortwave albedo (A). Radiative transfer model calculations are used in combination with measurements to separate the radiative effect of A (Delta SWA), wv (Delta SWwv), and aerosols (Delta SW tau) in modulating SW in cloud-free conditions. The shortwave radiation at the surface is mainly affected by water vapour absorption, which produces a reduction of SW as low as -100 Wm(-2) (-18%). The seasonal change of A produces an increase of SW by up to +25 Wm(-2) (+4.5%). The annual mean radiative effect is estimated to be -(21-22) Wm(-2) for wv, and +(2-3) Wm(-2) for A. An increase by +0.065 cm in the annual mean wv, to which corresponds an absolute increase in Delta SWwv by 0.93 Wm(-2) (4.3%), has been observed to occur between 2007 and 2010. In the same period, the annual mean A has decreased by -0.027, with a corresponding decrease in Delta SWA by 0.41 Wm(-2) (-14.9%). Atmospheric aerosols produce a reduction of SW as low as -32 Wm(-2) (-6.7%). The instantaneous aerosol radiative forcing (RF tau) reaches values of -28 Wm(-2) and shows a strong dependency on surface albedo. The derived radiative forcing efficiency (FE tau) for solar zenith angles between 55A degrees and 70A degrees is estimated to be (-120.6 +/- A 4.3) for 0.1 < A < 0.2, and (-41.2 +/- A 1.6) Wm(-2) for 0.5 < A < 0.6. C1 [Di Biagio, C.; di Sarra, A.] ENEA, Lab Earth Observat & Anal, I-00123 Rome, Italy. [Di Biagio, C.] Univ Siena, Dept Earth Sci, I-53100 Siena, Italy. [Eriksen, P.] DMI, Danish Climate Ctr, DK-2100 Copenhagen, Denmark. [Ascanius, S. E.] DMI, Qaanaaq, Greenland. [Muscari, G.] INGV, I-00143 Rome, Italy. [Holben, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Di Biagio, C (reprint author), ENEA, Lab Earth Observat & Anal, Via Anguillarese 301, I-00123 Rome, Italy. EM claudia.dibiagio@enea.it; alcide.disarra@enea.it; pe@dmi.dk; geobsthl@greennet.gl; giovanni.muscari@ingv.it; brent@aeronet.gsfc.nasa.gov RI di Sarra, Alcide/J-1491-2016 OI di Sarra, Alcide/0000-0002-2405-2898 FU project PRIN ("Dirigibile Italia''); Italian Ministry for University and Research; Italian Antarctic Program FX This work was supported by the project PRIN 2007 ("Dirigibile Italia''), funded by the Italian Ministry for University and Research, and by the Italian Antarctic Program. MODIS data are distributed by the Land Processes Distributed Active Archive Center (LP DAAC), located at the US Geological Survey (USGS) Earth Resources Observation and Science (EROS) Center (lpdaac.usgs.gov). We thank two anonymous reviewers for their helpful comments. NR 57 TC 6 Z9 6 U1 0 U2 25 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 AUG PY 2012 VL 39 IS 3-4 BP 953 EP 969 DI 10.1007/s00382-011-1280-1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 985MQ UT WOS:000307271200027 ER PT J AU Duren, RM Miller, CE AF Duren, Riley M. Miller, Charles E. TI COMMENTARY: Measuring the carbon emissions of megacities SO NATURE CLIMATE CHANGE LA English DT Editorial Material C1 [Duren, Riley M.; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91030 USA. RP Duren, RM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91030 USA. EM Riley.M.Duren@jpl.nasa.gov NR 16 TC 38 Z9 38 U1 5 U2 41 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 AUG PY 2012 VL 2 IS 8 BP 560 EP 562 PG 3 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 986TU UT WOS:000307369300004 ER PT J AU Petherick, A Rosenzweig, C AF Petherick, Anna Rosenzweig, Cynthia TI Agricultural futures SO NATURE CLIMATE CHANGE LA English DT Editorial Material C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, Climate Impacts Grp, New York, NY 10025 USA. NR 0 TC 0 Z9 0 U1 1 U2 8 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 AUG PY 2012 VL 2 IS 8 BP 567 EP 567 PG 1 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 986TU UT WOS:000307369300007 ER PT J AU Vogt, SS Butler, RP Haghighipour, N AF Vogt, S. S. Butler, R. P. Haghighipour, N. TI GJ 581 update: Additional evidence for a Super-Earth in the habitable zone SO ASTRONOMISCHE NACHRICHTEN LA English DT Editorial Material DE methods: numerical; planetary systems; stars: individual (GJ 581; HIP 74995); techniques: radial velocities ID M-CIRCLE-PLUS; SYSTEM; PLANETS AB We present an analysis of the significantly expanded HARPS 2011 radial velocity data set for GJ 581 that was presented by Forveille et al. (2011). Our analysis reaches substantially different conclusions regarding the evidence for a Super-Earth-mass planet in the star's Habitable Zone. We were able to reproduce their reported ?2? and RMS values only after removing some outliers from their models and refitting the trimmed down RV set. A suite of 4000 N-body simulations of their Keplerian model all resulted in unstable systems and revealed that their reported 3.6s detection of e = 0.32 for the eccentricity of GJ 581e is manifestly incompatible with the system's dynamical stability. Furthermore, their Keplerian model, when integrated only over the time baseline of the observations, significantly increases the ?2? and demonstrates the need for including non-Keplerian orbital precession when modeling this system. We find that a four-planet model with all of the planets on circular or nearly circular orbits provides both an excellent self-consistent fit to their RV data and also results in a very stable configuration. The periodogram of the residuals to a 4-planet all-circular-orbit model reveals significant peaks that suggest one or more additional planets in this system. We conclude that the present 240-point HARPS data set, when analyzed in its entirety, and modeled with fully self-consistent stable orbits, by and of itself does offer significant support for a fifth signal in the data with a period near 32 days. This signal has a false alarm probability of <4% and is consistent with a planet of minimum mass 2.2 M?, orbiting squarely in the star's habitable zone at 0.13 AU, where liquid water on planetary surfaces is a distinct possibility ((c) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [Vogt, S. S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Butler, R. P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, N.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Vogt, SS (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. EM vogt@ucolick.org RI Butler, Robert/B-1125-2009 NR 20 TC 23 Z9 23 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD AUG PY 2012 VL 333 IS 7 BP 561 EP 575 DI 10.1002/asna.201211707 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 981XE UT WOS:000307005200004 ER PT J AU Ackermann, M Ajello, M Baldini, L Barbiellini, G Baring, MG Bechtol, K Bellazzini, R Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bottacini, E Bouvier, A Brigida, M Buehler, R Buson, S Caliandro, GA Cameron, RA Cecchi, C Charles, E Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Cutini, S D'Ammando, F de Palma, F Dermer, CD Silva, EDE Drell, PS Drlica-Wagner, A Favuzzi, C Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Granot, J Grenier, IA Grove, JE Hadasch, D Hanabata, Y Harding, AK Hays, E Horan, D Johannesson, G Kataoka, J Knodlseder, J Kocevski, D Kuss, M Lande, J Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN McEnery, J McGlynn, S Michelson, PF Mitthumsiri, W Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Norris, JP Nuss, E Nymark, T Ohsugi, T Okumura, A Omodei, N Orlando, E Panetta, JH Parent, D Pelassa, V Pesce-Rollins, M Piron, F Pivato, G Racusin, JL Raino, S Rando, R Razzaque, S Reimer, A Reimer, O Ritz, S Ryde, F Sgro, C Siskind, EJ Sonbas, E Spandre, G Spinelli, P Stamatikos, M Stawarz, E Suson, DJ Takahashi, H Tanaka, T Thayer, JG Thayer, JB Tibaldo, L Tinivella, M Tosti, G Uehara, T Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Connaughton, V Briggs, MS Guirec, S Goldstein, A Burgess, JM Bhat, PN Bissaldi, E Camero-Arranz, A Fishman, J Fitzpatrick, G Foley, S Gruber, D Jenke, P Kippen, RM Kouveliotou, C McBreen, S Meegan, C Paciesas, WS Preece, R Rau, A Tierney, D van der Horst, AJ von Kienlin, A Wilson-Hodge, C Xiong, S AF Ackermann, M. Ajello, M. Baldini, L. Barbiellini, G. Baring, M. G. Bechtol, K. Bellazzini, R. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bottacini, E. Bouvier, A. Brigida, M. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cutini, S. D'Ammando, F. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Granot, J. Grenier, I. A. Grove, J. E. Hadasch, D. Hanabata, Y. Harding, A. K. Hays, E. Horan, D. Johannesson, G. Kataoka, J. Knoedlseder, J. Kocevski, D. Kuss, M. Lande, J. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. McEnery, J. McGlynn, S. Michelson, P. F. Mitthumsiri, W. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Norris, J. P. Nuss, E. Nymark, T. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Panetta, J. H. Parent, D. Pelassa, V. Pesce-Rollins, M. Piron, F. Pivato, G. Racusin, J. L. Raino, S. Rando, R. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Ryde, F. Sgro, C. Siskind, E. J. Sonbas, E. Spandre, G. Spinelli, P. Stamatikos, M. Stawarz, Eukasz Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Tibaldo, L. Tinivella, M. Tosti, G. Uehara, T. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Connaughton, V. Briggs, M. S. Guirec, S. Goldstein, A. Burgess, J. M. Bhat, P. N. Bissaldi, E. Camero-Arranz, A. Fishman, J. Fitzpatrick, G. Foley, S. Gruber, D. Jenke, P. Kippen, R. M. Kouveliotou, C. McBreen, S. Meegan, C. Paciesas, W. S. Preece, R. Rau, A. Tierney, D. van der Horst, A. J. von Kienlin, A. Wilson-Hodge, C. Xiong, S. CA Fermi Large Area Telescope Team Fermi Gamma-ray Burst Monitor Team TI CONSTRAINING THE HIGH-ENERGY EMISSION FROM GAMMA-RAY BURSTS WITH FERMI SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma rays: general ID LARGE-AREA TELESCOPE; SPECTRAL COMPONENT; BATSE OBSERVATIONS; LORENTZ FACTORS; GRB 100724B; CATALOG; LIMITS; HARD; SPECTROSCOPY; PHOTONS AB We examine 288 gamma-ray bursts (GRBs) detected by the Fermi Gamma-ray Space Telescope's Gamma-ray Burst Monitor (GBM) that fell within the field of view of Fermi's Large Area Telescope (LAT) during the first 2.5 years of observations, which showed no evidence for emission above 100 MeV. We report the photon flux upper limits in the 0.1-10 GeV range during the prompt emission phase as well as for fixed 30 s and 100 s integrations starting from the trigger time for each burst. We compare these limits with the fluxes that would be expected from extrapolations of spectral fits presented in the first GBM spectral catalog and infer that roughly half of the GBM-detected bursts either require spectral breaks between the GBM and LAT energy bands or have intrinsically steeper spectra above the peak of the nu F-nu spectra (E-pk). In order to distinguish between these two scenarios, we perform joint GBM and LAT spectral fits to the 30 brightest GBM-detected bursts and find that a majority of these bursts are indeed softer above E-pk than would be inferred from fitting the GBM data alone. Approximately 20% of this spectroscopic subsample show statistically significant evidence for a cutoff in their high-energy spectra, which if assumed to be due to gamma gamma attenuation, places limits on the maximum Lorentz factor associated with the relativistic outflow producing this emission. All of these latter bursts have maximum Lorentz factor estimates that are well below the minimum Lorentz factors calculated for LAT-detected GRBs, revealing a wide distribution in the bulk Lorentz factor of GRB outflows and indicating that LAT-detected bursts may represent the high end of this distribution. C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Glanzman, T.; Kocevski, D.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Panetta, J. H.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ajello, M.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Glanzman, T.; Kocevski, D.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Panetta, J. H.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Universe & Particules Montpellier, CNRS, IN2P3, Montpellier, France. [Chekhtman, A.; D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy. [D'Ammando, F.] INAF Ist Astrofis Spaziale Fis & Cosm, I-00133 Rome, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Fukazawa, Y.; Hanabata, Y.; Uehara, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gehrels, N.; Harding, A. K.; Hays, E.; McEnery, J.; Racusin, J. L.; Sonbas, E.; Stamatikos, M.; Guirec, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Grenier, I. A.; Naumann-Godo, M.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [McGlynn, S.] Tech Univ Munich, D-85748 Garching, Germany. [Moretti, E.; Nymark, T.; Ryde, F.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Moretti, E.; Nymark, T.; Ryde, F.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.; Stawarz, Eukasz] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Orlando, E.; Foley, S.; Gruber, D.; McBreen, S.; Rau, A.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Parent, D.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Bouvier, A.; Pelassa, V.; Connaughton, V.; Briggs, M. S.; Goldstein, A.; Burgess, J. M.; Bhat, P. N.; Fishman, J.; Paciesas, W. S.; Preece, R.; Xiong, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Reimer, A.; Reimer, O.; Bissaldi, E.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Bissaldi, E.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Sonbas, E.] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey. [Sonbas, E.; Camero-Arranz, A.; Meegan, C.] USRA, Columbia, MD 21044 USA. [Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Stawarz, Eukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Camero-Arranz, A.; Jenke, P.; Kouveliotou, C.; van der Horst, A. J.; Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Fitzpatrick, G.; Foley, S.; McBreen, S.; Tierney, D.] Natl Univ Ireland Univ Coll Dublin, Dublin 4, Ireland. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Connaughton, V.; Briggs, M. S.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM valerie@nasa.gov; jchiang@slac.stanford.edu; kocevski@slac.stanford.edu; moretti@particle.kth.se; connauv@uah.edu; michael.briggs@nasa.gov RI Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Orlando, E/R-5594-2016; Hays, Elizabeth/D-3257-2012; Johannesson, Gudlaugur/O-8741-2015; Morselli, Aldo/G-6769-2011; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Racusin, Judith/D-2935-2012; Harding, Alice/D-3160-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013 OI Moretti, Elena/0000-0001-5477-9097; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Bissaldi, Elisabetta/0000-0001-9935-8106; Giordano, Francesco/0000-0002-8651-2394; Preece, Robert/0000-0003-1626-7335; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Burgess, James/0000-0003-3345-9515; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852; McBreen, Sheila/0000-0002-1477-618X; Mazziotta, Mario Nicola/0000-0001-9325-4672; Johannesson, Gudlaugur/0000-0003-1458-7036; Morselli, Aldo/0000-0002-7704-9553; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 43 TC 33 Z9 33 U1 0 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 121 DI 10.1088/0004-637X/754/2/121 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700042 ER PT J AU De Buizer, JM Bartkiewicz, A Szymczak, M AF De Buizer, James M. Bartkiewicz, Anna Szymczak, Marian TI TESTING THE HYPOTHESIS THAT METHANOL MASER RINGS TRACE CIRCUMSTELLAR DISKS: HIGH-RESOLUTION NEAR-INFRARED AND MID-INFRARED IMAGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; masers; stars: formation ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; VLBI OBSERVATIONS; GHZ; MODELS; I.; DISTRIBUTIONS; PARAMETERS; ACCRETION; OUTFLOWS AB Milliarcsecond very long baseline interferometry maps of regions containing 6.7 GHz methanol maser emission have lead to the recent discovery of ring-like distributions of maser spots and the plausible hypothesis that they may be tracing circumstellar disks around forming high-mass stars. We aimed to test this hypothesis by imaging these regions in the near-and mid-infrared at high spatial resolution and compare the observed emission to the expected infrared morphologies as inferred from the geometries of the maser rings. In the near-infrared we used the Gemini North adaptive optics system of ALTAIR/NIRI, while in the mid-infrared we used the combination of the Gemini South instrument T-ReCS and super-resolution techniques. Resultant images had a resolution of similar to 150 mas in both the near-infrared and mid-infrared. We discuss the expected distribution of circumstellar material around young and massive accreting (proto) stars and what infrared emission geometries would be expected for the different maser ring orientations under the assumption that the masers are coming from within circumstellar disks. Based upon the observed infrared emission geometries for the four targets in our sample and the results of spectral energy distribution modeling of the massive young stellar objects associated with the maser rings, we do not find compelling evidence in support of the hypothesis that methanol masers rings reside in circumstellar disks. C1 [De Buizer, James M.] NASA, Stratospher Observ Infrared Astronomy USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bartkiewicz, Anna; Szymczak, Marian] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. RP De Buizer, JM (reprint author), NASA, Stratospher Observ Infrared Astronomy USRA, Ames Res Ctr, MS N232-12, Moffett Field, CA 94035 USA. EM jdebuizer@sofia.usra.edu RI Bartkiewicz, Anna/D-6212-2014; Szymczak, Marian/D-6773-2014 FU Polish Ministry of Science and Higher Education [N203 386937]; Nicolaus Copernicus University [378-A] FX A.B. and M.S. acknowledge support by the Polish Ministry of Science and Higher Education through grant N203 386937. A.B. also acknowledges support by the Nicolaus Copernicus University grant 378-A (2010). We thank Dr. Eric Greisen from NRAO and Dr. Jagadheep Pandian from University of Hawaii for fruitful discussions. NR 39 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 149 DI 10.1088/0004-637X/754/2/149 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700070 ER PT J AU Ford, J Hildebrandt, H Van Waerbeke, L Leauthaud, A Capak, P Finoguenov, A Tanaka, M George, MR Rhodes, J AF Ford, Jes Hildebrandt, Hendrik Van Waerbeke, Ludovic Leauthaud, Alexie Capak, Peter Finoguenov, Alexis Tanaka, Masayuki George, Matthew R. Rhodes, Jason TI MAGNIFICATION BY GALAXY GROUP DARK MATTER HALOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: photometry ID LYMAN-BREAK GALAXIES; LENSING MAGNIFICATION; COSMIC MAGNIFICATION; LUMINOSITY FUNCTION; DEEP FIELDS; WEAK; SHEAR; MASS; CHALLENGE; ACCURACY AB We report on the detection of gravitational lensing magnification by a population of galaxy groups, at a significance level of 4.9s. Using X-ray-selected groups in the COSMOS 1.64 deg(2) field, and high-redshift Lyman break galaxies as sources, we measure a lensing-induced angular cross-correlation between the samples. After satisfying consistency checks that demonstrate we have indeed detected a magnification signal, and are not suffering from contamination by physical overlap of samples, we proceed to implement an optimally weighted cross-correlation function to further boost the signal to noise of the measurement. Interpreting this optimally weighted measurement allows us to study properties of the lensing groups. We model the full distribution of group masses using a composite-halo approach, considering both the singular isothermal sphere and Navarro-Frenk-White profiles, and find our best-fit values to be consistent with those recovered using the weak-lensing shear technique. We argue that future weak-lensing studies will need to incorporate magnification along with shear, both to reduce residual systematics and to make full use of all available source information, in an effort to maximize scientific yield of the observations. C1 [Ford, Jes; Hildebrandt, Hendrik; Van Waerbeke, Ludovic] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hildebrandt, Hendrik] Argelander Inst Astron, D-53121 Bonn, Germany. [Leauthaud, Alexie; Tanaka, Masayuki] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778582, Japan. [Capak, Peter] CALTECH, NASA Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Finoguenov, Alexis] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Finoguenov, Alexis] Univ Maryland Baltimore Cty, Ctr Space Sci Technol, Baltimore, MD 21250 USA. [George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [George, Matthew R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rhodes, Jason] CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA. RP Ford, J (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. OI Ford, Jes/0000-0002-2946-3776 FU JPL [1394704]; NSERC; CIfAR; Marie Curie IOF [252760]; CITA National Fellowship; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan FX The authors thank Fabian Schmidt and Martha Milkeraitis for useful discussions related to this work. J.F. was supported by JPL grant No. 1394704, and is now supported by NSERC and CIfAR. H.H. is supported by the Marie Curie IOF 252760 and by a CITA National Fellowship. This work was performed in part at JPL, run by Caltech under a contract for NASA. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. This work is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, and on observations made with the NASA/ESA Hubble Space Telescope. 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 is also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. NR 33 TC 29 Z9 29 U1 1 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 AUG 1 PY 2012 VL 754 IS 2 AR 143 DI 10.1088/0004-637X/754/2/143 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700064 ER PT J AU Hayashida, M Madejski, GM Nalewajko, K Sikora, M Wehrle, AE Ogle, P Collmar, W Larsson, S Fukazawa, Y Itoh, R Chiang, J Stawarz, L Blandford, RD Richards, JL Max-Moerbeck, W Readhead, A Buehler, R Cavazzuti, E Ciprini, S Gehrels, N Reimer, A Szostek, A Tanaka, T Tosti, G Uchiyama, Y Kawabata, KS Kino, M Sakimoto, K Sasada, M Sato, S Uemura, M Yamanaka, M Greiner, J Kruehler, T Rossi, A Macquart, JP Bock, DCJ Villata, M Raiteri, CM Agudo, I Aller, HD Aller, MF Arkharov, AA Bach, U Benitez, E Berdyugin, A Blinov, DA Blumenthal, K Bottcher, M Buemi, CS Carosati, D Chen, WP Di Paola, A Dolci, M Efimova, NV Forne, E Gomez, JL Gurwell, MA Heidt, J Hiriart, D Jordan, B Jorstad, SG Joshi, M Kimeridze, G Konstantinova, TS Kopatskaya, EN Koptelova, E Kurtanidze, OM Lahteenmaki, A Lamerato, A Larionov, VM Larionova, EG Larionova, LV Leto, P Lindfors, E Marscher, AP McHardy, IM Molina, SN Morozova, DA Nikolashvili, MG Nilsson, K Reinthal, R Roustazadeh, P Sakamoto, T Sigua, LA Sillanpaa, A Takalo, L Tammi, J Taylor, B Tornikoski, M Trigilio, C Troitsky, IS Umana, G AF Hayashida, M. Madejski, G. M. Nalewajko, K. Sikora, M. Wehrle, A. E. Ogle, P. Collmar, W. Larsson, S. Fukazawa, Y. Itoh, R. Chiang, J. Stawarz, L. Blandford, R. D. Richards, J. L. Max-Moerbeck, W. Readhead, A. Buehler, R. Cavazzuti, E. Ciprini, S. Gehrels, N. Reimer, A. Szostek, A. Tanaka, T. Tosti, G. Uchiyama, Y. Kawabata, K. S. Kino, M. Sakimoto, K. Sasada, M. Sato, S. Uemura, M. Yamanaka, M. Greiner, J. Kruehler, T. Rossi, A. Macquart, J. P. Bock, D. C. -J. Villata, M. Raiteri, C. M. Agudo, I. Aller, H. D. Aller, M. F. Arkharov, A. A. Bach, U. Benitez, E. Berdyugin, A. Blinov, D. A. Blumenthal, K. Boettcher, M. Buemi, C. S. Carosati, D. Chen, W. P. Di Paola, A. Dolci, M. Efimova, N. V. Forne, E. Gomez, J. L. Gurwell, M. A. Heidt, J. Hiriart, D. Jordan, B. Jorstad, S. G. Joshi, M. Kimeridze, G. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kurtanidze, O. M. Lahteenmaki, A. Lamerato, A. Larionov, V. M. Larionova, E. G. Larionova, L. V. Leto, P. Lindfors, E. Marscher, A. P. McHardy, I. M. Molina, S. N. Morozova, D. A. Nikolashvili, M. G. Nilsson, K. Reinthal, R. Roustazadeh, P. Sakamoto, T. Sigua, L. A. Sillanpaa, A. Takalo, L. Tammi, J. Taylor, B. Tornikoski, M. Trigilio, C. Troitsky, I. S. Umana, G. TI THE STRUCTURE AND EMISSION MODEL OF THE RELATIVISTIC JET IN THE QUASAR 3C 279 INFERRED FROM RADIO TO HIGH-ENERGY gamma-RAY OBSERVATIONS IN 2008-2010 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (3C 279); radiation mechanisms: non-thermal; X-rays: galaxies ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; MULTIBAND IMAGING PHOTOMETER; FERMI-DETECTED BLAZARS; MULTIWAVELENGTH OBSERVATIONS; SPACE-TELESCOPE; ABSOLUTE CALIBRATION; GASP-WEBT; X-RAY; ELECTROMAGNETIC-SPECTRUM AB We present time-resolved broadband observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. While investigating the previously reported gamma-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears to be delayed with respect to the gamma-ray emission by about 10 days. X-ray observations reveal a pair of "isolated" flares separated by similar to 90 days, with only weak gamma-ray/optical counterparts. The spectral structure measured by Spitzer reveals a synchrotron component peaking in the mid-infrared band with a sharp break at the far-infrared band during the gamma-ray flare, while the peak appears in the millimeter (mm)/submillimeter (sub-mm) band in the low state. Selected spectral energy distributions are fitted with leptonic models including Comptonization of external radiation produced in a dusty torus or the broad-line region. Adopting the interpretation of the polarization swing involving propagation of the emitting region along a curved trajectory, we can explain the evolution of the broadband spectra during the gamma-ray flaring event by a shift of its location from similar to 1 pc to similar to 4 pc from the central black hole. On the other hand, if the gamma-ray flare is generated instead at sub-pc distance from the central black hole, the far-infrared break can be explained by synchrotron self-absorption. We also model the low spectral state, dominated by the mm/sub-mm peaking synchrotron component, and suggest that the corresponding inverse-Compton component explains the steady X-ray emission. C1 [Hayashida, M.; Madejski, G. M.; Chiang, J.; Blandford, R. D.; Buehler, R.; Reimer, A.; Szostek, A.; Tanaka, T.; Uchiyama, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Hayashida, M.] Kyoto Univ, Dept Astron, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Nalewajko, K.] Univ Colorado, Boulder, CO 80309 USA. [Nalewajko, K.; Sikora, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Wehrle, A. E.] Space Sci Inst, Boulder, CO 80301 USA. [Ogle, P.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Collmar, W.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Larsson, S.] Stockholm Univ, 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. [Fukazawa, Y.; Itoh, R.; Sakimoto, K.; Sasada, M.; Yamanaka, M.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.; Szostek, A.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Richards, J. L.; Max-Moerbeck, W.; Readhead, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Cavazzuti, E.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Ciprini, S.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Gehrels, N.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Kawabata, K. S.; Uemura, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Kino, M.; Sato, S.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Rossi, A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Macquart, J. P.] Curtin Univ Technol, Bentley, WA 6845, Australia. [Macquart, J. P.] Int Ctr Radio Astron Res, Bentley, WA 6845, Australia. [Bock, D. C. -J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Villata, M.; Raiteri, C. M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy. [Agudo, I.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Agudo, I.; Blumenthal, K.; Jorstad, S. G.; Joshi, M.; Marscher, A. P.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Arkharov, A. A.; Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia. [Bach, U.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Benitez, E.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Berdyugin, A.; Lindfors, E.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland. [Blinov, D. A.; Efimova, N. V.; Jorstad, S. G.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Boettcher, M.; Lamerato, A.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain. [Carosati, D.] TNG Fdn Galileo Galilei, INAF, La Palma, Spain. [Chen, W. P.; Koptelova, E.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taiwan. [Dolci, M.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Roma, Italy. [Dolci, M.] Osservatorio Astron Collurania Vincenzo Cerruli, INAF, I-64100 Teramo, Italy. [Forne, E.] Agrupacio Astron Sabadell, Sabadell 08206, Spain. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heidt, J.] Heidelberg Univ, ZAH, Landesternwarte, D-69117 Heidelberg, Germany. [Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Kimeridze, G.; Kurtanidze, O. M.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia. [Koptelova, E.] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Lahteenmaki, A.; Tammi, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [McHardy, I. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikiio, Finland. [Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Hayashida, M (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, 2575 Sand Hill Rd,M-S 29, Menlo Pk, CA 94025 USA. EM mahaya@slac.stanford.edu; madejski@slac.stanford.edu; knalew@Colorado.edu; sikora@camk.edu.pl RI Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Molina, Sol Natalia/F-9968-2015; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Macquart, Jean-Pierre/B-5306-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova, Elena/H-7287-2013; Efimova, Natalia/I-2196-2013; Blinov, Dmitry/G-9925-2013 OI Umana, Grazia/0000-0002-6972-8388; Leto, Paolo/0000-0003-4864-2806; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Dolci, Mauro/0000-0001-8000-5642; Buemi, Carla Simona/0000-0002-7288-4613; Villata, Massimo/0000-0003-1743-6946; Larionova, Liudmila/0000-0002-0274-1481; Molina, Sol Natalia/0000-0002-4112-2157; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova, Elena/0000-0002-2471-6500; Efimova, Natalia/0000-0002-8071-4753; Blinov, Dmitry/0000-0003-0611-5784 FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Smithsonian Institution; Academia Sinica; Russian RFBR foundation [09-02-00092]; MICIIN (Spain) [AYA2010-14844]; CEIC (Andalucia) [P09-FQM-4784]; Academy of Finland [212656, 210338, 121148]; NASA Fermi GI [NNX08AV65G, NNX08AV61G, NNX09AT99G, NNX09AU10G]; NSF [AST-0907893, AST-0607523]; BU; Lowell Observatory; UK Science and Technology Facilities Council; Georgian National Science Foundation [GNSF/ST09/521 4-320]; NASA; NASA [NNX09AU16G, NNX10AP16G, NNX11AO13G]; University of Michigan; Japan Society for the Promotion of Science for Young Scientists; Polish MNiSW [N N203 301635, N N203 386337]; Polish ASTRONET [621/E-78/SN-0068/2007]; Polish NCN [DEC-2011/01/B/ST9/04845] 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 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 St. Petersburg University team acknowledges support from the Russian RFBR foundation via grant 09-02-00092. AZT-24 observations are made within an agreement between Pulkovo, Rome, and Teramo observatories. This paper is partly based on observations carried out at the German-Spanish Calar Alto Observatory, which is jointly operated by the MPIA and the IAA-CSIC. Acquisition of the MAPCAT data is supported in part by MICIIN (Spain) grant and AYA2010-14844, and by CEIC (Andalucia) grant P09-FQM-4784. The Metsaahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). The Medicina and Noto telescopes are operated by INAF-Istituto di Radioastronomia. The research at Boston University was supported by NASA Fermi GI grants NNX08AV65G, NNX08AV61G, NNX09AT99G, and NNX09AU10G, and NSF grant AST-0907893. The PRISM camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, with funding from the UK Science and Technology Facilities Council. The Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST09/521 4-320. The research at the University of Michigan has been funded by a series of grants from NASA and from the NSF. Specific grant numbers are NASA grants NNX09AU16G, NNX10AP16G, NNX11AO13G, and NSF grant AST-0607523. Funding for the operation of UMRAO was provided by the University of Michigan.; M.H. is supported by the Research Fellowships of the Japan Society for the Promotion of Science for Young Scientists. This work was partially supported by the Polish MNiSW grants N N203 301635 and N N203 386337, the Polish ASTRONET grant 621/E-78/SN-0068/2007, and the Polish NCN grant DEC-2011/01/B/ST9/04845. NR 99 TC 58 Z9 58 U1 0 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 114 DI 10.1088/0004-637X/754/2/114 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700035 ER PT J AU Kahler, SW Akiyama, S Gopalswamy, N AF Kahler, S. W. Akiyama, S. Gopalswamy, N. TI DEFLECTIONS OF FAST CORONAL MASS EJECTIONS AND THE PROPERTIES OF ASSOCIATED SOLAR ENERGETIC PARTICLE EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: particle emission ID FAST-WIND REGIONS; SPACE WEATHER; SEP EVENTS; HOLES; HELIOSPHERE; STEREO; SUN; ACCELERATION; PROPAGATION; INTENSITIES AB The onset times and peak intensities of solar energetic particle (SEP) events at Earth have long been thought to be influenced by the open magnetic fields of coronal holes (CHs). The original idea was that a CH lying between the solar SEP source region and the magnetic footpoint of the 1 AU observer would result in a delay in onset and/or a decrease in the peak intensity of that SEP event. Recently, Gopalswamy et al. showed that CHs near coronal mass ejection (CME) source regions can deflect fast CMEs from their expected trajectories in space, explaining the appearance of driverless shocks at 1 AU from CMEs ejected near solar central meridian (CM). This suggests that SEP events originating in CME-driven shocks may show variations attributable to CH deflections of the CME trajectories. Here, we use a CH magnetic force parameter to examine possible effects of CHs on the timing and intensities of 41 observed gradual E similar to 20 MeV SEP events with CME source regions within 20 degrees of CM. We find no systematic CH effects on SEP event intensity profiles. Furthermore, we find no correlation between the CME leading-edge measured position angles and SEP event properties, suggesting that the widths of CME-driven shock sources of the SEPs are much larger than the CMEs. Independently of the SEP event properties, we do find evidence for significant CME deflections by CH fields in these events. C1 [Kahler, S. W.] USAF, Res Lab, Space Vehicles Directorate, Kirtland AFB, NM 87117 USA. [Akiyama, S.] Catholic Univ Amer, Inst Astrophy & Computat Sci, Washington, DC 20064 USA. [Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kahler, SW (reprint author), USAF, Res Lab, Space Vehicles Directorate, 3550 Aberdeen Ave, Kirtland AFB, NM 87117 USA. EM AFRL.RVB.PA@kirtland.af.mil OI Gopalswamy, Nat/0000-0001-5894-9954 FU AFOSR [2301RDZ4]; NASA's LWS TRT FX S. Kahler was funded by AFOSR Task 2301RDZ4. N. Gopalswamy and S. Akiyama were supported by NASA's LWS TR&T program. CME data were taken from the CDAW LASCO catalog. This CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between ESA and NASA. NR 48 TC 7 Z9 7 U1 7 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 100 DI 10.1088/0004-637X/754/2/100 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700021 ER PT J AU Marley, MS Saumon, D Cushing, M Ackerman, AS Fortney, JJ Freedman, R AF Marley, Mark S. Saumon, Didier Cushing, Michael Ackerman, Andrew S. Fortney, Jonathan J. Freedman, Richard TI MASSES, RADII, AND CLOUD PROPERTIES OF THE HR 8799 PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; planetary systems; stars: atmospheres; stars: individual (HR 8799); stars: low-mass ID DWARF GLIESE 229B; EXTRASOLAR GIANT PLANETS; STAR ADAPTIVE OPTICS; COOL BROWN DWARF; T-DWARFS; L/T TRANSITION; MU-M; SPACE-TELESCOPE; ATMOSPHERIC PROPERTIES; CHEMICAL-EQUILIBRIUM AB The near-infrared colors of the planets directly imaged around the A star HR 8799 are much redder than most field brown dwarfs of the same effective temperature. Previous theoretical studies of these objects have concluded that the atmospheres of planets b, c, and d are unusually cloudy or have unusual cloud properties. Some studies have also found that the inferred radii of some or all of the planets disagree with expectations of standard giant planet evolution models. Here, we compare the available data to the predictions of our own set of atmospheric and evolution models that have been extensively tested against observations of field L and T dwarfs, including the reddest L dwarfs. Unlike some previous studies, we require mutually consistent choices for effective temperature, gravity, cloud properties, and planetary radius. This procedure thus yields plausible values for the masses, effective temperatures, and cloud properties of all three planets. We find that the cloud properties of the HR 8799 planets are not unusual but rather follow previously recognized trends, including a gravity dependence on the temperature of the L to T spectral transition-some reasons for which we discuss. We find that the inferred mass of planet b is highly sensitive to whether or not we include the H- and the K-band spectrum in our analysis. Solutions for planets c and d are consistent with the generally accepted constraints on the age of the primary star and orbital dynamics. We also confirm that, like in L and T dwarfs and solar system giant planets, non-equilibrium chemistry driven by atmospheric mixing is also important for these objects. Given the preponderance of data suggesting that the L to T spectral type transition is gravity dependent, we present an exploratory evolution calculation that accounts for this effect. Finally we recompute the bolometric luminosity of all three planets. C1 [Marley, Mark S.; Freedman, Richard] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Cushing, Michael] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Freedman, Richard] SETI Inst, Moffett Field, CA 94035 USA. RP Marley, MS (reprint author), NASA, Ames Res Ctr, MS-245-3, Moffett Field, CA 94035 USA. EM Mark.S.Marley@NASA.gov; dsaumon@lanl.gov; michael.cushing@utoledo.edu; andrew.ackerman@nasa.gov; jfortney@ucolick.org; freedman@darkstar.arc.nasa.gov RI Ackerman, Andrew/D-4433-2012; Marley, Mark/I-4704-2013; OI Ackerman, Andrew/0000-0003-0254-6253; Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943 FU National Aeronautics and Space Administration; NASA Postdoctoral Program at the Jet Propulsion Laboratory; W. M. Keck Foundation; Spitzer Space telescope Theoretical Research Program FX We thank Travis Barman and Bruce Macintosh for helpful conversations and Travis Barman for a particularly helpful review. This material is based upon work supported by the National Aeronautics and Space Administration through the Planetary Atmospheres and Astrophysics Theory Programs as well as the Spitzer Space telescope Theoretical Research Program. This research was supported in part 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 is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Observations used here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. 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 113 TC 91 Z9 91 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 135 DI 10.1088/0004-637X/754/2/135 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700056 ER PT J AU Marrone, DP Smith, GP Okabe, N Bonamente, M Carlstrom, JE Culverhouse, TL Gralla, M Greer, CH Hasler, N Hawkins, D Hennessy, R Joy, M Lamb, JW Leitch, EM Martino, R Mazzotta, P Miller, A Mroczkowski, T Muchovej, S Plagge, T Pryke, C Sanderson, AJR Takada, M Woody, D Zhang, YY AF Marrone, Daniel P. Smith, Graham P. Okabe, Nobuhiro Bonamente, Massimiliano Carlstrom, John E. Culverhouse, Thomas L. Gralla, Megan Greer, Christopher H. Hasler, Nicole Hawkins, David Hennessy, Ryan Joy, Marshall Lamb, James W. Leitch, Erik M. Martino, Rossella Mazzotta, Pasquale Miller, Amber Mroczkowski, Tony Muchovej, Stephen Plagge, Thomas Pryke, Clem Sanderson, Alastair J. R. Takada, Masahiro Woody, David Zhang, Yuying TI LoCuSS: THE SUNYAEV-ZEL'DOVICH EFFECT AND WEAK-LENSING MASS SCALING RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: intracluster medium; gravitational lensing: weak ID LUMINOUS GALAXY CLUSTERS; SOUTH-POLE TELESCOPE; X-RAY-PROPERTIES; DARK-MATTER; INTRACLUSTER MEDIUM; COSMOLOGICAL CONSTRAINTS; PARAMETER-ESTIMATION; LINEAR-REGRESSION; ASTRONOMICAL DATA; PRESSURE PROFILE AB We present the first weak-lensing-based scaling relation between galaxy cluster mass, M-WL, and integrated Compton parameter Y-sph. Observations of 18 galaxy clusters at z similar or equal to 0.2 were obtained with the Subaru 8.2 m telescope and the Sunyaev-Zel'dovich Array. The M-WL-Y-sph scaling relations, measured at Delta = 500, 1000, and 2500 rho(c), are consistent in slope and normalization with previous results derived under the assumption of hydrostatic equilibrium (HSE). We find an intrinsic scatter in M-WL at fixed Y-sph of 20%, larger than both previous measurements of M-HSE-Y-sph scatter as well as the scatter in true mass at fixed Y-sph found in simulations. Moreover, the scatter in our lensing-based scaling relations is morphology dependent, with 30%-40% larger M-WL for undisturbed compared to disturbed clusters at the same Y-sph at r(500). Further examination suggests that the segregation may be explained by the inability of our spherical lens models to faithfully describe the three-dimensional structure of the clusters, in particular, the structure along the line of sight. We find that the ellipticity of the brightest cluster galaxy, a proxy for halo orientation, correlates well with the offset in mass from the mean scaling relation, which supports this picture. This provides empirical evidence that line-of-sight projection effects are an important systematic uncertainty in lensing-based scaling relations. C1 [Marrone, Daniel P.; Carlstrom, John E.; Gralla, Megan; Greer, Christopher H.; Hennessy, Ryan; Leitch, Erik M.; Plagge, Thomas] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Smith, Graham P.; Sanderson, Alastair J. R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Okabe, Nobuhiro] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Okabe, Nobuhiro] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Bonamente, Massimiliano; Hasler, Nicole] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Bonamente, Massimiliano; Joy, Marshall] NASA, George C Marshall Space Flight Ctr, Space Sci VP62, Huntsville, AL 35812 USA. [Carlstrom, John E.; Gralla, Megan; Greer, Christopher H.; Hennessy, Ryan; Leitch, Erik M.; Plagge, Thomas] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, John E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, John E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Culverhouse, Thomas L.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Culverhouse, Thomas L.; Hawkins, David; Lamb, James W.; Muchovej, Stephen; Woody, David] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA. [Martino, Rossella; Mazzotta, Pasquale] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Miller, Amber] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Miller, Amber] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Mroczkowski, Tony] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Pryke, Clem] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Takada, Masahiro] Univ Tokyo, IPMU, Chiba 2778582, Japan. [Zhang, Yuying] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Marrone, DP (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM dmarrone@email.arizona.edu RI Takada, Masahiro/A-4364-2011; Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; Marrone, Daniel/0000-0002-2367-1080; Mroczkowski, Tony/0000-0003-3816-5372 FU Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; states of California, Illinois, and Maryland; National Science Foundation [AST-0838187, PHY-0114422, PHY-0551164]; NASA [HST-HF-51259.01, PF0-110077]; Royal Society; Tohoku University; Ministry of Education, Culture, Sports, Science, and Technology of Japan; German BMBF through the Verbundforschung [50 OR 1005]; [0740099]; [18072001] FX We thank Daisuke Nagai, Laurie Shaw, Neelima Sehgal, and Rebecca Stanek for providing their simulated scaling relations. We are grateful to Gus Evrard, Andrey Kravtsov, Matthew Becker, and Bradford Benson for comments that have improved this manuscript. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, including grant AST-0838187 at the University of Chicago, and by the CARMA partner universities. Partial support is provided by NSF Physics Frontier Center Grant PHY-0114422 to the Kavli Institute of Cosmological Physics. D. P. M. was supported for part of this work by NASA through Hubble Fellowship Grant HST-HF-51259.01. He acknowledges the Kavli Institute for Theoretical Physics for its hospitality during part of this research, supported by NSF Grant PHY-0551164. G. P. S. acknowledges support from the Royal Society. Support for T. M. was provided by NASA through the Einstein Fellowship Program, grant PF0-110077. N. O. was partially supported by a Grant-in-Aid (0740099), and this work was supported by the programs "Weaving Science Web beyond Particle-Matter Hierarchy" in Tohoku University and "Probing the Dark Energy through an Extremely Wide and Deep Survey with Subaru Telescope" (18072001), all of which are funded by the Ministry of Education, Culture, Sports, Science, and Technology of Japan. Y.Y.Z. acknowledges support from the German BMBF through the Verbundforschung under grant No. 50 OR 1005. NR 96 TC 54 Z9 54 U1 0 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 119 DI 10.1088/0004-637X/754/2/119 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700040 ER PT J AU Mei, S Stanford, SA Holden, BP Raichoor, A Postman, M Nakata, F Finoguenov, A Ford, HC Illingworth, GD Kodama, T Rosati, P Tanaka, M Huertas-Company, M Rettura, A Shankar, F Carrasco, ER Demarco, R Eisenhardt, P Jee, MJ Koyama, Y White, RL AF Mei, Simona Stanford, S. Adam Holden, Brad P. Raichoor, Anand Postman, Marc Nakata, Fumiaki Finoguenov, Alexis Ford, Holland C. Illingworth, Garth D. Kodama, Tadayuki Rosati, Piero Tanaka, Masayuki Huertas-Company, Marc Rettura, Alessandro Shankar, Francesco Carrasco, Eleazar R. Demarco, Ricardo Eisenhardt, Peter Jee, Myungkook J. Koyama, Yusei White, Richard L. TI EARLY-TYPE GALAXIES AT z=1.3. I. THE LYNX SUPERCLUSTER: CLUSTER AND GROUPS AT z=1.3. MORPHOLOGY AND COLOR-MAGNITUDE RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (the Lynx cluster); galaxies: evolution; galaxies: high-redshift; galaxies: stellar content; galaxies: structure ID HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; DIGITAL SKY SURVEY; SUPPORT VECTOR MACHINES; PHOTON IMAGING CAMERA; SEEING LIMITED IMAGES; WIDE-FIELD SURVEY; LESS-THAN 2; ELLIPTIC GALAXIES; XMM-NEWTON AB We confirm the detection of three groups in the Lynx supercluster, at z approximate to 1.3 through spectroscopic follow-up and X-ray imaging, and we give estimates for their redshifts and masses. We study the properties of the group galaxies compared to the two central clusters, RX J0849+4452 and RX J0848+4453. Using spectroscopic follow-up and multi-wavelength photometric redshifts, we select 89 galaxies in the clusters, of which 41 are spectroscopically confirmed, and 74 galaxies in the groups, of which 25 are spectroscopically confirmed. We morphologically classify galaxies by visual inspection, noting that our early-type galaxy (ETG) sample would have been contaminated at the 30%-40% level by simple automated classification methods (e.g., based on Sersic index). In luminosity-selected samples, both clusters and groups show high fractions of bulge-dominated galaxies with a diffuse component that we visually identified as a disk and which we classified as bulge-dominated spirals, e.g., Sas. The ETG fractions never rise above approximate to 50% in the clusters, which is low compared to the fractions observed in other massive clusters at z approximate to 1. In the groups, ETG fractions never exceed approximate to 25%>. However, overall bulge-dominated galaxy fractions (ETG plus Sas) are similar to those observed for ETGs in clusters at z similar to 1. Bulge-dominated galaxies visually classified as spirals might also be ETGs with tidal features or merger remnants. They are mainly red and passive, and span a large range in luminosity. Their star formation seems to have been quenched before experiencing a morphological transformation. Because their fractions is smaller at lower redshifts, they might be the spiral population that evolves into ETGs. For mass-selected samples of galaxies with masses M > 10(10.6) M-circle dot within Sigma > 500 Mpc(-2,) the ETG and overall bulge-dominated galaxy fractions show no significant evolution with respect to local clusters, suggesting that morphological transformations might occur at lower masses and densities. The ETG mass-size relation shows evolution toward smaller sizes at higher redshift in both cluster and groups, while the late-type mass-size relation matches that observed locally. When compared to the clusters, the group ETG red sequence shows lower zero points (at similar to 2 sigma) and large scatters, both expected to be an indication of a younger galaxy population. However, we show that any allowed difference between the age in groups and clusters would be small when compared to the difference in age in galaxies of different masses. C1 [Mei, Simona; Raichoor, Anand; Huertas-Company, Marc] Observ Paris, Sect Meudon, GEPI, F-92190 Meudon, France. [Mei, Simona; Huertas-Company, Marc] Univ Paris Denis Diderot, Dept Phys, F-75205 Paris 13, France. [Mei, Simona] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Stanford, S. Adam; Rettura, Alessandro; Jee, Myungkook J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. Adam] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Holden, Brad P.; Illingworth, Garth D.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95065 USA. [Raichoor, Anand] INAF Osservatorio Astron Brera, I-20121 Milan, Italy. [Postman, Marc; White, Richard L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Nakata, Fumiaki; Kodama, Tadayuki] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Finoguenov, Alexis] Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. [Ford, Holland C.; Rettura, Alessandro] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kodama, Tadayuki] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Rosati, Piero] European S Observ, D-85748 Garching, Germany. [Tanaka, Masayuki; Koyama, Yusei] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Rettura, Alessandro] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Shankar, Francesco] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Carrasco, Eleazar R.] So Operat Ctr, Gemini Observ, La Serena, Chile. [Demarco, Ricardo] Univ Concepcion, Dept Astron, Concepcion, Chile. [Eisenhardt, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mei, S (reprint author), Observ Paris, Sect Meudon, GEPI, 5 Pl J Janssen, F-92190 Meudon, France. OI Postman, Marc/0000-0002-9365-7989; Carrasco, Eleazar Rodrigo/0000-0002-7272-9234 FU NASA HST grant [GO-10574.01-A]; Spitzer program [20694]; W.M. Keck Foundation; BASAL Center for Astrophysics and Associated Technologies (CATA); FONDECYT Grant [1100540] FX ACS was developed under NASA contract NAS 5-32865. This research has been supported by the NASA HST grant GO-10574.01-A and Spitzer program 20694. The Space Telescope Science Institute is operated by AURA Inc., under NASA contract NAS5-26555. 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 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 data were based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil), Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina), and Gemini Science Program ID: GN-2006A-Q-78. R.D. gratefully acknowledges the support provided by the BASAL Center for Astrophysics and Associated Technologies (CATA) and by FONDECYT Grant No. 1100540. We thank the anonymous referee for the very constructive suggestions and Shannon Patel for useful discussions. NR 109 TC 27 Z9 27 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 AUG 1 PY 2012 VL 754 IS 2 AR 141 DI 10.1088/0004-637X/754/2/141 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700062 ER PT J AU Ofman, L Wang, TJ Davila, JM AF Ofman, L. Wang, T. J. Davila, J. M. TI SLOW MAGNETOSONIC WAVES AND FAST FLOWS IN ACTIVE REGION LOOPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: activity; Sun: corona; Sun: flares; Sun: oscillations; Sun: UV radiation; waves ID SOLAR CORONAL LOOP; MAGNETOACOUSTIC WAVES; STANDING WAVES; SPECTROSCOPIC OBSERVATIONS; NUMERICAL SIMULATIONS; OSCILLATIONS; HOT; SUMER; SEISMOLOGY; SIGNATURE AB Recent extreme ultraviolet spectroscopic observations indicate that slow magnetosonic waves are present in active region (AR) loops. Some of the spectral data were also interpreted as evidence of fast (similar to 100-300 km s(-1)) quasi-periodic flows. We have performed three-dimensional magnetohydrodynamic (3D MHD) modeling of a bipolar AR that contains impulsively generated waves and flows in coronal loops. The model AR is initiated with a dipole magnetic field and gravitationally stratified density, with an upflow-driven steadily or periodically in localized regions at the footpoints of magnetic loops. The resulting flows along the magnetic field lines of the AR produce higher density loops compared to the surrounding plasma by injection of material into the flux tubes and the establishment of siphon flow. We find that the impulsive onset of flows with subsonic speeds result in the excitation of damped slow magnetosonic waves that propagate along the loops and coupled nonlinearly driven fast-mode waves. The phase speed of the slow magnetosonic waves is close to the coronal sound speed. When the amplitude of the driving pulses is increased we find that slow shock-like wave trains are produced. When the upflows are driven periodically, undamped oscillations are produced with periods determined by the periodicity of the upflows. Based on the results of the 3D MHD model we suggest that the observed slow magnetosonic waves and persistent upflows may be produced by the same impulsive events at the bases of ARs. C1 [Ofman, L.; Wang, T. J.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Ofman, L.; Wang, T. J.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ofman, L (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. FU NASA [NNX12AB34G, NNX08AV88G, NNX09AG10G, NNX10AN10G, NNX08AE44G] FX We acknowledge support by NASA grant NNX12AB34G. L.O. was also supported by NASA grants NNX08AV88G, NNX09AG10G, and NNX10AN10G. T.J.W. was also supported by NASA Grants NNX10AN10G and NNX08AE44G. We acknowledge the use of computer resources at NASAs Ames Research Center advanced supercomputing facility. NR 43 TC 33 Z9 33 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 111 DI 10.1088/0004-637X/754/2/111 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700032 ER PT J AU Tappe, A Rho, J Boersma, C Micelotta, ER AF Tappe, A. Rho, J. Boersma, C. Micelotta, E. R. TI POLYCYCLIC AROMATIC HYDROCARBON PROCESSING IN THE BLAST WAVE OF THE SUPERNOVA REMNANT N132D SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: individual objects (N132D); ISM: molecules; ISM: supernova remnants; shock waves ID SPITZER-SPACE-TELESCOPE; RICH PROTOPLANETARY NEBULAE; INFRARED SPECTROGRAPH; MAGELLANIC CLOUD; DUST DESTRUCTION; MU-M; EMISSION; SPECTROSCOPY; G11.2-0.3; YOUNG AB We present Spitzer Infrared Spectrograph 14-36 mu m mapping observations of the supernova remnant N132D in the Large Magellanic Cloud. This study focuses on the processing of polycyclic aromatic hydrocarbons (PAHs) that we previously identified in the southern blast wave. The mid-infrared spectra show strong continuum emission from shock-heated dust and a unique, nearly featureless plateau in the 15-20 mu m region, which we attribute to PAH molecules. The typical PAH emission bands observed in the surrounding interstellar medium ahead of the blast wave disappear, which indicates shock processing of PAH molecules. The PAH plateau appears most strongly at the outer edge of the blast wave and coincides with diffuse X-ray emission that precedes the brightest X-ray and optical filaments. This suggests that PAH molecules in the surrounding medium are swept up and processed in the hot gas of the blast wave shock, where they survive the harsh conditions long enough to be detected. We also observe a broad emission feature at 20 mu m appearing with the PAH plateau. We speculate that this feature is either due to FeO dust grains or connected to the processing of PAHs in the supernova blast wave shock. C1 [Tappe, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rho, J.] NASA, SOFIA Sci Mission Operat USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Micelotta, E. R.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. RP Tappe, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-72, Cambridge, MA 02138 USA. EM atappe@cfa.harvard.edu RI Boersma, Christiaan/L-7696-2014; OI Boersma, Christiaan/0000-0002-4836-217X; Micelotta, Elisabetta/0000-0002-6555-5109 FU NASA [NNX10AQ84G]; NASA at Ames Research Center 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 a contract with NASA. Support for this work was provided by NASA funding through the Spitzer GO program and the Astrophysics Data Analysis Program NNX10AQ84G (awarded to J. Rho). C. Boersma is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 33 TC 5 Z9 5 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 132 DI 10.1088/0004-637X/754/2/132 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700053 ER PT J AU Tibbs, CT Paladini, R Compiegne, M Dickinson, C Alves, MIR Flagey, N Shenoy, S Noriega-Crespo, A Carey, S Casassus, S Davies, RD Davis, RJ Molinari, S Elia, D Pestalozzi, M Schisano, E AF Tibbs, C. T. Paladini, R. Compiegne, M. Dickinson, C. Alves, M. I. R. Flagey, N. Shenoy, S. Noriega-Crespo, A. Carey, S. Casassus, S. Davies, R. D. Davis, R. J. Molinari, S. Elia, D. Pestalozzi, M. Schisano, E. TI A MULTI-WAVELENGTH INVESTIGATION OF RCW175: AN H II REGION HARBORING SPINNING DUST EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; H II regions; ISM: abundances; ISM: individual objects (RCW175, G29.1-0.7, G29.0-0.6) ID ANOMALOUS MICROWAVE EMISSION; RADIO-CONTINUUM SURVEY; MASSIVE-STAR-FORMATION; GALACTIC PLANE SURVEY; SPECTRAL ENERGY-DISTRIBUTION; FORMATION RATE INDICATORS; HII-REGIONS; ANISOTROPY-PROBE; MILKY-WAY; COSMOSOMAS EXPERIMENT AB Using infrared, radio continuum, and spectral observations, we performed a detailed investigation of the H II region RCW175. We determined that RCW175, which actually consists of two separate H II regions, G29.1-0.7 and G29.0-0.6, is located at a distance of 3.2 +/- 0.2 kpc. Based on the observations we infer that the more compact G29.0-0.6 is less evolved than G29.1-0.7 and was possibly produced as a result of the expansion of G29.1-0.7 into the surrounding interstellar medium. We compute a star formation rate for RCW175 of (12.6 +/- 1.9) x 10(-5) M-circle dot yr(-1), and identified six possible young stellar object candidates within its vicinity. Additionally, we estimate that RCW175 contains a total dust mass of 215 +/- 53 M-circle dot. RCW175 has previously been identified as a source of anomalous microwave emission (AME), an excess of emission at centimeter wavelengths often attributed to electric dipole radiation from the smallest dust grains. We find that the AME previously detected in RCW175 is not correlated with the smallest dust grains (polycyclic aromatic hydrocarbons or small carbonaceous dust grains), but rather with the exciting radiation field within the region. This is a similar result to that found in the Perseus molecular cloud, another region which harbors AME, suggesting that the radiation field may play a pivotal role in the production of this new Galactic emission mechanism. Finally, we suggest that these observations may hint at the importance of understanding the role played by the major gas ions in spinning dust models. C1 [Tibbs, C. T.; Compiegne, M.; Carey, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Paladini, R.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Compiegne, M.] Univ Lille 1, CNRS, INSU, Lab Opt Atmospher,UMR8518, F-59655 Villeneuve Dascq, France. [Dickinson, C.; Davies, R. D.; Davis, R. J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Alves, M. I. R.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Flagey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Shenoy, S.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Noriega-Crespo, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Casassus, S.] Univ Chile, Dept Astron, Santiago, Chile. [Molinari, S.; Elia, D.; Pestalozzi, M.; Schisano, E.] Ist Fis Spazio Interplanetario, INAF, I-00133 Rome, Italy. RP Tibbs, CT (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM ctibbs@ipac.caltech.edu RI Casassus, Simon/I-8609-2016; Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Elia, Davide/0000-0002-9120-5890 FU NASA/ADP ROSES [09-ADP09-0059]; NASA; National Science Foundation [AST-9800334, AST-0098562, AST-0100793, AST-0228993, AST-0507657]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA) FX We thank the anonymous referee for providing useful comments that improved the content of this paper. We also thank Mark Calabretta and Lister Staveley-Smith for help with the RRL data. This work has been performed within the framework of a NASA/ADP ROSES-2009 grant No. 09-ADP09-0059. C.D. acknowledges an STFC Advanced Fellowship and EU Marie Curie IRG grant under the FP7. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the National Science Foundation under grants AST-9800334, AST-0098562, AST-0100793, AST-0228993, and AST-0507657. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including 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 97 TC 24 Z9 24 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 94 DI 10.1088/0004-637X/754/2/94 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700015 ER PT J AU Solomon, SC Burns, AG Emery, BA Mlynczak, MG Qian, LY Wang, WB Weimer, DR Wiltberger, M AF Solomon, Stanley C. Burns, Alan G. Emery, Barbara A. Mlynczak, Martin G. Qian, Liying Wang, Wenbin Weimer, Daniel R. Wiltberger, Michael TI Modeling studies of the impact of high-speed streams and co-rotating interaction regions on the thermosphere-ionosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND STREAMS; GENERAL-CIRCULATION MODEL; ADVANCED COMPOSITION EXPLORER; WHOLE HELIOSPHERE INTERVAL; GEOMAGNETIC-ACTIVITY; CORONAL HOLES; ACCELEROMETER DATA; SABER EXPERIMENT; AURORAL MODEL; EUV FLUX AB Changes in the thermosphere-ionosphere system caused by high-speed streams in the solar wind, and the co-rotating interaction regions they engender, are studied using a combination of model simulations and data analysis. The magnetospheric responses to these structures and consequent ionospheric drivers are simulated using the numerical Coupled Magnetosphere-Ionosphere-Thermosphere model and the empirical Weimer 2005 model, finding that the interplanetary magnetic field (IMF) is more important than solar wind speed and density per se in controlling magnetosphere-ionosphere coupling. The NCAR Thermosphere-Ionosphere-Electrodynamics General Circulation Model is then employed to calculate neutral density, nitric oxide cooling, and electron density, for comparison to space-based measurements from the STAR instrument on the CHAMP satellite, the SABER instrument on the TIMED satellite, and GPS occultations from the COSMIC mission, respectively. The recurrent, periodic changes observed under solar minimum conditions during 2008, and particularly during the Whole Heliospheric Interval (March-April of 2008), are simulated by the model and compared to these measurements. Numerical experiments were conducted to elucidate the mechanisms of solar wind and IMF forcing, setting the solar wind speed and density to nominal values, smoothing the IMF, and also setting it to zero. The results confirm the importance of IMF variations, particularly its north-south component (B-z), but also show that when the average B-z values are negative (southward), the interaction with increased solar wind speed amplifies the magnetosphere-ionosphere-thermosphere response. Conversely, during events when B-z is on average positive (northward), even large increases in solar wind speed have small effects on the system. C1 [Solomon, Stanley C.; Burns, Alan G.; Emery, Barbara A.; Qian, Liying; Wang, Wenbin; Wiltberger, Michael] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Weimer, Daniel R.] Virginia Polytech Inst & State Univ, Natl Inst Aerosp, Blacksburg, VA 24061 USA. RP Solomon, SC (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, 3080 Ctr Green Dr, Boulder, CO 80307 USA. EM stans@ucar.edu RI Wiltberger, Michael/B-8781-2008; Solomon, Stanley/J-4847-2012; Mlynczak, Martin/K-3396-2012; Wang, Wenbin/G-2596-2013; Qian, Liying/D-9236-2013; Burns, Alan/L-1547-2013 OI Wiltberger, Michael/0000-0002-4844-3148; Solomon, Stanley/0000-0002-5291-3034; Wang, Wenbin/0000-0002-6287-4542; Qian, Liying/0000-0003-2430-1388; FU Center for Integrated Space Weather Modeling under NSF [ATM-0120950]; NASA [NNX08AQ31G, NNX10AF21G]; National Science Foundation FX The authors thank Eric Sutton for providing the CHAMP neutral density data and the UCAR COSMIC team for providing the electron density data. The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. This research was supported by the Center for Integrated Space Weather Modeling under NSF agreement ATM-0120950 and by NASA grants NNX08AQ31G and NNX10AF21G to the National Center for Atmospheric Research. NCAR is supported by the National Science Foundation. NR 93 TC 25 Z9 25 U1 1 U2 25 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 AUG 1 PY 2012 VL 117 AR A00L11 DI 10.1029/2011JA017417 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 984HR UT WOS:000307181200001 ER PT J AU Jacobson, NS Myers, DL Harder, BJ AF Jacobson, Nathan S. Myers, Dwight L. Harder, Bryan J. TI Active oxidation of silicon carbide SO MATERIALS AT HIGH TEMPERATURES LA English DT Article DE active oxidation; silicon carbide; oxide scale ID TO-PASSIVE TRANSITION; ELEVATED-TEMPERATURES; KINETICS; AIR; ENVIRONMENTS; CORROSION; FLOW AB The active oxidation of SiC has been studied at 1390 and 1490 degrees C, paying particular attention to the active-to-passive and passive-to-active transition points. First the active-to-passive transition for pure silicon was studied at 1290 degrees C. The beginning of passivity is characterized by micron-sized SiO2 rod formation on the surface due to the oxidation of SiO(g), consistent with other investigators. These rods were not observed in the active-to-passive transition for SiC; but they were observed in the passive-to-active transition for SiC. This type of microstructure yields information about the breakdown of the passive film. Unlike pure silicon, at a fixed temperature a substantial difference in the transition oxygen pressure for the active-to-passive and passive-to-active transitions was not observed for SiC. This is due to the fact that both processes are controlled by SiC/SiO2 interfacial reactions. Studies were also conducted on active oxidation C1 [Jacobson, Nathan S.; Harder, Bryan J.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Myers, Dwight L.] E Cent Univ, Dept Chem, Ada, OK 74820 USA. RP Jacobson, NS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM nathan.s.jacobson@nasa.gov NR 18 TC 0 Z9 0 U1 3 U2 13 PU SCIENCE REVIEWS 2000 LTD PI ST ALBANS PA PO BOX 314, ST ALBANS AL1 4ZG, HERTS, ENGLAND SN 0960-3409 J9 MATER HIGH TEMP JI Mater. High Temp. PD AUG PY 2012 VL 29 IS 3 BP 193 EP 198 DI 10.3184/096034012X13322284984793 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 981OC UT WOS:000306976700006 ER PT J AU Suess, M Greenhall, CA AF Suess, Matthias Greenhall, Charles A. TI Combined covariance reductions for Kalman filter composite clocks SO METROLOGIA LA English DT Article AB The impact of combining two covariance matrix reduction methods on the resulting Kalman filter timescale estimates and covariances is addressed. The Brown and Greenhall reduction operations commute, and the combination of both reductions gives the same Kalman filter estimates as the Greenhall reduction alone. The benefit of combining both methods is that the Greenhall reduced covariances are further reduced in the positive semi-definite sense. A numerical example demonstrates the combined reduction by calculating the trace of the original and reduced covariance matrices. It is pointed out that the corrected clock offsets can follow the system time offset with different precisions, but the mutual disagreements of the corrected time offsets (called synchronization error) can be identical. C1 [Suess, Matthias] German Aerosp Ctr, Oberpfaffenhoffen, Germany. [Greenhall, Charles A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Suess, M (reprint author), German Aerosp Ctr, Muenchener Str 20, Oberpfaffenhoffen, Germany. EM Matthias.suess@dlr.de; cgreenhall@jpl.nasa.gov FU National Aeronautics and Space Administration FX The authors would like to thank Demetrios Matsakis from United States Naval Observatory for helpful discussions and suggestions and the department of Navigation of the German Aerospace Center. The work of the second author was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 12 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0026-1394 J9 METROLOGIA JI Metrologia PD AUG PY 2012 VL 49 IS 4 BP 588 EP 596 DI 10.1088/0026-1394/49/4/588 PG 9 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 979PE UT WOS:000306831400023 ER PT J AU Feakins, SJ Warny, S Lee, JE AF Feakins, Sarah J. Warny, Sophie Lee, Jung-Eun TI Hydrologic cycling over Antarctica during the middle Miocene warming SO NATURE GEOSCIENCE LA English DT Article ID PALAEOCENE/EOCENE THERMAL MAXIMUM; ISOTOPIC COMPOSITION; EAST ANTARCTICA; CLIMATE; ICE; PRECIPITATION; HISTORY; WATER; CORE; GCM AB From 20 to 15 million years (Myr) ago, a period of global warmth reversed the previous ice growth on Antarctica, leading to the retreat of the West Antarctic Ice Sheet and the contraction of the East Antarctic Ice Sheet(1,2). Pollen recovered from the Antarctic shelf indicates the presence of substantial vegetation on the margins of Antarctica 15.7 Myr ago(3). However, the hydrologic regime that supported this vegetation is unclear. Here we combine leaf-wax hydrogen isotopes and pollen assemblages from Ross Sea sediments with model simulations to reconstruct vegetation, precipitation and temperature in Antarctica during the middle Miocene. Average leaf-wax stable hydrogen isotope (delta D) values from 20 to 15.5 Myr ago translate to average delta D values of -50 parts per thousand h for precipitation at the margins of Antarctica, higher than modern values. We find that vegetation persisted from 20 to 15.5 Myr ago, with peak expansions 16.4 and 15.7 Myr ago coinciding with peak global warmth(4) and vegetation growth(5). Our model experiments are consistent with a local moisture source in the Southern Ocean(6). Combining proxy measurements with climate simulations, we conclude that summer temperatures were about 11 degrees C warmer than today, and that there was a substantial increase in moisture delivery to the Antarctic coast. C1 [Feakins, Sarah J.] Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA. [Warny, Sophie] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. [Warny, Sophie] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Lee, Jung-Eun] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Feakins, SJ (reprint author), Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA. EM feakins@usc.edu RI Lee, Jung-Eun/F-8981-2012; Feakins, Sarah/K-4149-2012; Warny, Sophie/A-8226-2013 OI Feakins, Sarah/0000-0003-3434-2423; FU US National Science Foundation [ANT-0342484, 25-0550-0001-155, 25-0550-0001-137, ANT-1048343, EAR-090919, 0342484]; NASA ROSES Aura Science Team [NNH07ZDA001N-AST07-0069] FX This research used samples acquired by the ANDRILL project and provided by the Antarctic Marine Geology Research Facility at Florida State University. The ANDRILL project is a multinational collaboration involving the Antarctic programmes of Germany, Italy, New Zealand and the USA. The Antarctic Marine Geology Research Facility is sponsored by the US National Science Foundation. Financial support for this research was provided by the US National Science Foundation (ANT-0342484 to D. Harwood and R. Levy, subawards 25-0550-0001-155 to S.J.F. and 25-0550-0001-137 to S.W., ANT-1048343 to S.W. and EAR-090919 to P.Molnar for J-E.L.). This material is based on work supported by the US National Science Foundation under cooperative agreement no. 0342484 through subawards administered and issued by the ANDRILL Science Management Office at the University of Nebraska-Lincoln, as part of the ANDRILL US Science Support program. 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 US National Science Foundation. . We acknowledge laboratory assistance from M. Rincon, M. Cheetham, Z. Zhang and L. Foersterling and discussions with D. Harwood, A. Tripati, A. Kahmen, J. West, J. Tierney, P. Bart, R. Askin, H. Bao, A. Sessions, G. Schmidt and J. Hayes. The simulations were carried out on the Division of Geological and Planetary Sciences' Dell cluster at the California Institute of Technology, and J-E.L. thanks T.Schneider, T. Merlis, and Z. Tan for their help in incorporating isotopes into GRAM and support by the NASA ROSES Aura Science Team NNH07ZDA001N-AST07-0069. NR 30 TC 35 Z9 35 U1 2 U2 35 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 AUG PY 2012 VL 5 IS 8 BP 557 EP 560 DI 10.1038/NGEO1498 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 983DR UT WOS:000307099000013 ER PT J AU Singer, KN McKinnon, WB Schenk, PM Moore, JM AF Singer, Kelsi N. McKinnon, William B. Schenk, Paul M. Moore, Jeffery M. TI Massive ice avalanches on Iapetus mobilized by friction reduction during flash heating SO NATURE GEOSCIENCE LA English DT Article ID VALLES-MARINERIS; ACOUSTIC FLUIDIZATION; ALBEDO DICHOTOMY; LARGE LANDSLIDES; MARS; DEBRIS; STURZSTROMS; TOPOGRAPHY; VELOCITIES; MOVEMENTS AB Long-runout landslides are debris flows or avalanches that travel much farther than expected. They apparently exhibit friction coefficients much lower than either the static or sliding values that are generally accepted for geologic materials. Many friction-reduction mechanisms have been proposed for such landslides observed on Earth and Mars. Here we analyse images from the Cassini mission and report numerous long-runout landslides on Iapetus, an icy satellite of exceptional topographic relief. Its extremely cold, airless surface provides an excellent laboratory for studying long-runout landslides, as influence by trapped atmosphere or groundwater-two proposed friction-reduction mechanisms-is negligible. We use the ratio of drop height to runout length as an approximation for the friction coefficient of landslide material. We find that on Iapetus this ratio falls between 0.1 and 0.3, but does not decrease with increasing length as seen on Earth and Mars. We show that this lack of dependence is consistent with localized frictional heating in ice rubble such that sliding surfaces are slippery. Friction along tectonic faults on icy bodies may be similarly reduced. C1 [Singer, Kelsi N.; McKinnon, William B.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Singer, Kelsi N.; McKinnon, William B.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Schenk, Paul M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Moore, Jeffery M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Singer, KN (reprint author), Washington Univ, Dept Earth & Planetary Sci, 1 Brookings Dr, St Louis, MO 63130 USA. EM knsinger@wustl.edu FU NASA; Cassini Data Analysis Program; NESS FX This work was supported by grants from the NASA Planetary Geology and Geophysics Program (W. B. M.) and Cassini Data Analysis Program (J.M.M. and P. M. S.) and by a NESS Fellowship to K.N.S. We sincerely thank A. Lucas for comments that substantially improved this paper, and dedicate this work to the memory of R. Greeley. NR 46 TC 16 Z9 16 U1 2 U2 10 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 AUG PY 2012 VL 5 IS 8 BP 574 EP 578 DI 10.1038/NGEO1526 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 983DR UT WOS:000307099000017 ER PT J AU Tanaka, Z Perry, M Cooper, G Tang, SN McKay, CP Chen, B AF Tanaka, Zuki Perry, Meredith Cooper, George Tang, Suning McKay, Christopher P. Chen, Bin TI Near-Infrared (NIR) Raman Spectroscopy of Precambrian Carbonate Stromatolites with Post-Depositional Organic Inclusions SO APPLIED SPECTROSCOPY LA English DT Article DE Raman spectroscopy; Mars; Astrobiology; Stromatolites ID 1064 NM; EASTERN CALIFORNIA; MARS; MICROFOSSILS; SPECTRA; LIFE AB Raman spectroscopy has promising potential for future Mars missions as a non-contact detection technique for characterizing organic material and mineralogy. Such a capability will be useful for selecting samples for detailed analysis on a rover and for selecting samples for return to Earth. Stromatolites are important evidence for the earliest life on Earth and are promising targets for Mars investigations. Although constructed by microorganisms, stromatolites are organo-sedimentary structures that can be large enough to be discovered and investigated by a Mars rover. In this paper, we report the Raman spectroscopic investigations of the carbonate mineralogy and organic layering in a Precambrian (similar to 1.5 Cyr old) stromatolite from the Crystal Spring Formation of Southern California. Ultraviolet (UV: 266 nm), visible (514 nm, 633 nm), and near-infrared (NIR: 785 nm, 1064 nm) Raman spectra are presented. We conclude that 1064 nm excitation is the optimal excitation wavelength for avoiding intrinsic fluorescence and detecting organic carbon within the carbonate matrix. Our results confirm that NIR Raman spectroscopy has important applications for future Mars missions. C1 [Tanaka, Zuki; Chen, Bin] UC Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95060 USA. [Tanaka, Zuki; Cooper, George; McKay, Christopher P.; Chen, Bin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Perry, Meredith] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. [Tang, Suning] Crystal Res Inc, Fremont, CA 95439 USA. RP Chen, B (reprint author), UC Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95060 USA. EM Bin.Chen-1@NASA.gov FU NASA; Planetary Instrument Definition and Development; Astrobiology Institute; Small Business Innovative Research grant; Pennsylvania Space Grant Consortium FX The authors would like to acknowledge Bayspec Inc. for the construction of the spectrometer. SEM and EDS instruments were operated at the Materials Analysis for Collaborative Science facility at NASA Ames Research Center. Funding for this research was provided by NASA Graduate Student Research Program (ZT), Planetary Instrument Definition and Development (BC and CPM), Astrobiology Institute and Pennsylvania Space Grant Consortium (MP), and Small Business Innovative Research (ST) grant supports. NR 32 TC 4 Z9 4 U1 4 U2 20 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0003-7028 EI 1943-3530 J9 APPL SPECTROSC JI Appl. Spectrosc. PD AUG PY 2012 VL 66 IS 8 BP 911 EP 916 DI 10.1366/11-06523 PG 6 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA 978DK UT WOS:000306720600007 PM 22800768 ER PT J AU Adams, ER Ciardi, DR Dupree, AK Gautier, TN Kulesa, C McCarthy, D AF Adams, E. R. Ciardi, D. R. Dupree, A. K. Gautier, T. N., III Kulesa, C. McCarthy, D. TI ADAPTIVE OPTICS IMAGES OF KEPLER OBJECTS OF INTEREST SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; instrumentation: adaptive optics; planets and satellites: detection ID PLANET CANDIDATES; MULTIPLE SYSTEM; STAR; CAMERA AB All transiting planets are at risk of contamination by blends with nearby, unresolved stars. Blends dilute the transit signal, causing the planet to appear smaller than it really is, or produce a false-positive detection when the target star is blended with eclipsing binary stars. This paper reports on high spatial-resolution adaptive optics images of 90 Kepler planetary candidates. Companion stars are detected as close as 0.'' 1 from the target star. Images were taken in the near-infrared (J and Ks bands) with ARIES on the MMT and PHARO on the Palomar Hale 200 inch telescope. Most objects (60%) have at least one star within 6 '' separation and a magnitude difference of 9. Eighteen objects (20%) have at least one companion within 2 '' of the target star; six companions (7%) are closer than 0.'' 5. Most of these companions were previously unknown, and the associated planetary candidates should receive additional scrutiny. Limits are placed on the presence of additional companions for every system observed, which can be used to validate planets statistically using the BLENDER method. Validation is particularly critical for low-mass, potentially Earth-like worlds, which are not detectable with current-generation radial velocity techniques. High-resolution images are thus a crucial component of any transit follow-up program. C1 [Adams, E. R.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ciardi, D. R.] NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Gautier, T. N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kulesa, C.; McCarthy, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Adams, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Ciardi, David/0000-0002-5741-3047 NR 20 TC 61 Z9 61 U1 0 U2 4 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 AUG PY 2012 VL 144 IS 2 AR 42 DI 10.1088/0004-6256/144/2/42 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600013 ER PT J AU Dieterich, SB Henry, TJ Golimowski, DA Krist, JE Tanner, AM AF Dieterich, Sergio B. Henry, Todd J. Golimowski, David A. Krist, John E. Tanner, Angelle M. TI THE SOLAR NEIGHBORHOOD. XXVIII. THE MULTIPLICITY FRACTION OF NEARBY STARS FROM 5 TO 70 AU AND THE BROWN DWARF DESERT AROUND M DWARFS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: close; brown dwarfs; infrared: stars; solar neighborhood; stars: low-mass; stars: statistics ID LOW-MASS STARS; LUMINOSITY FUNCTION; T-DWARFS; SUBSTELLAR COMPANIONS; CORONAGRAPHIC SURVEY; EXTRASOLAR PLANETS; ULTRACOOL DWARFS; UPPER-SCORPIUS; YOUNG STARS; SKY SURVEY AB We report on our analysis of Hubble Space Telescope/NICMOS snapshot high-resolution images of 255 stars in 201 systems within similar to 10 pc of the Sun. Photometry was obtained through filters F110W, F180M, F207M, and F222M using NICMOS Camera 2. These filters were selected to permit clear identification of cool brown dwarfs through methane contrast imaging. With a plate scale of 76 mas pixel(-1), NICMOS can easily resolve binaries with subarcsecond separations in the 19 '' 5 x 19 '' 5 field of view. We previously reported five companions to nearby M and L dwarfs from this search. No new companions were discovered during the second phase of data analysis presented here, confirming that stellar/substellar binaries are rare. We establish magnitude and separation limits for which companions can be ruled out for each star in the sample, and then perform a comprehensive sensitivity and completeness analysis for the subsample of 138 M dwarfs in 126 systems. We calculate a multiplicity fraction of 0.0(-0.0)(+3.5)% for L companions to M dwarfs in the separation range of 5-70 AU, and 2.3(-0.7)(+5.0)% for L and T companions to M dwarfs in the separation range of 10- 70 AU. We also discuss trends in the color-magnitude diagrams using various color combinations and present astrometry for 19 multiple systems in our sample. Considering these results and results from several other studies, we argue that the so-called brown dwarf desert extends to binary systems with low-mass primaries and is largely independent of primary mass, mass ratio, and separations. While focusing on companion properties, we discuss how the qualitative agreement between observed companion mass functions and initial mass functions suggests that the paucity of brown dwarfs in either population may be due to a common cause and not due to binary formation mechanisms. C1 [Dieterich, Sergio B.; Henry, Todd J.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Golimowski, David A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Krist, John E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tanner, Angelle M.] Mississippi State Univ, Dept Phys & Astron, Mississippi State, MS 39762 USA. RP Dieterich, SB (reprint author), Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. EM dieterich@chara.gsu.edu FU NASA from the Space Telescope Science Institute (STScI) [HST-GO-07420, HST-GO-07894, HST-GO-09485] FX The authors thank Russel White, Deepak Raghavan, and Adam Burgasser for useful conversations. We thank our anonymous referee for many insightful comments that greatly improved the paper. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with HST programs 7420, 7894, and 9485. Support for these observations was provided by NASA through grants HST-GO-07420, HST-GO-07894, and HST-GO-09485 from the Space Telescope Science Institute (STScI). NR 61 TC 38 Z9 38 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2012 VL 144 IS 2 AR 64 DI 10.1088/0004-6256/144/2/64 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600035 ER PT J AU Fuse, C Marcum, P Fanelli, M AF Fuse, C. Marcum, P. Fanelli, M. TI EXTREMELY ISOLATED EARLY-TYPE GALAXIES IN THE SLOAN DIGITAL SKY SURVEY. I. THE SAMPLE SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: photometry ID SURVEY PHOTOMETRIC SYSTEM; ELLIPTIC GALAXIES; AMIGA SAMPLE; X-RAY; CATALOG; FIELD; ENVIRONMENTS; DENSITY AB We describe the properties of a sample of extremely isolated early-type galaxies (IEGs) selected from the spectroscopic Sloan Digital Sky Survey. Sample galaxies are isolated from nearest neighbors more luminous than M-V = -16.5 by a minimum distance corresponding to 2.5 Mpc and 350 km s (1) in redshift space. The candidate IEGs exhibit a number of unusual features as compared to bulge-dominated galaxies in cluster and group environments, including fainter luminosities, blue colors suggesting possible recent star formation, and smaller physical sizes. The paper is the first in a series analyzing this isolated galaxy sample. C1 [Fuse, C.] Rollins Coll, Dept Phys, Winter Pk, FL 32789 USA. [Fuse, C.; Marcum, P.; Fanelli, M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA. [Fanelli, M.] NASA, Ames Res Ctr, BAER Inst, Mountain View, CA 94035 USA. RP Fuse, C (reprint author), Rollins Coll, Dept Phys, Winter Pk, FL 32789 USA. EM cfuse@rollins.edu; pamela.m.marcum@nasa.gov; michael.n.fanelli@nasa.gov FU NASA Astrophysics Data and Analysis Program [NNG05C53G]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX This research has made use of the NASA/IPAC Extragalactic Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for this project was partially provided through NASA Astrophysics Data and Analysis Program grant NNG05C53G to the Texas Christian University (TCU). We gratefully acknowledge additional support through the NASA/Texas Space Grant Consortium Fellowship. This research has been used as partial fulfillment of the PhD degree at TCU (C.F.). We also acknowledge the extensive comments from the reviewer, which greatly aided the final version of this paper.; 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/. NR 43 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2012 VL 144 IS 2 AR 57 DI 10.1088/0004-6256/144/2/57 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600028 ER PT J AU Hinse, TC Gozdziewski, K Lee, JW Haghighipour, N Lee, CU AF Hinse, Tobias Cornelius Gozdziewski, Krzysztof Lee, Jae Woo Haghighipour, Nader Lee, Chung-Uk TI THE PROPOSED QUADRUPLE SYSTEM SZ HERCULIS: REVISED LITE MODEL AND ORBITAL STABILITY STUDY SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: individual (SZ Herculis) ID CIRCUMBINARY PLANETS; COMPANION; STARS; DWARF AB In a recent study, Lee et al. presented new photometric follow-up timing observations of the semidetached binary system SZ Herculis and proposed the existence of two hierarchical cirumbinary companions. Based on the light-travel time effect, the two low-mass M-dwarf companions are found to orbit the binary pair on moderate to high eccentric orbits. The derived periods of these two companions are close to a 2: 1 mean-motion orbital resonance. We have studied the stability of the system using the osculating orbital elements as presented by Lee et al. Results indicate an orbit-crossing architecture exhibiting short-term dynamical instabilities leading to the escape of one of the proposed companions. We have examined the system's underlying model parameter space by following a Monte Carlo approach and found an improved fit to the timing data. A study of the stability of our best-fitting orbits also indicates that the proposed system is generally unstable. If the observed anomalous timing variations of the binary period is due to additional circumbinary companions, then the resulting system should exhibit a long-term stable orbital configuration much different from the orbits suggested by Lee et al. We, therefore, suggest that based on Newtonian-dynamical considerations, the proposed quadruple system cannot exist. To uncover the true nature of the observed period variations of this system, we recommend future photometric follow-up observations that could further constrain eclipse-timing variations and/or refine light-travel time models. C1 [Hinse, Tobias Cornelius; Lee, Jae Woo; Lee, Chung-Uk] Korea Astron & Space Sci Inst, Adv Astron & Space Sci Div, Taejon 305348, South Korea. [Hinse, Tobias Cornelius] Armagh Observ, Armagh BT61 9DG, North Ireland. [Gozdziewski, Krzysztof] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Haghighipour, Nader] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, Nader] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. RP Hinse, TC (reprint author), Korea Astron & Space Sci Inst, Adv Astron & Space Sci Div, Taejon 305348, South Korea. EM tchinse@gmail.com RI Gozdziewski, Krzysztof/D-6291-2014 OI Gozdziewski, Krzysztof/0000-0002-8705-1577 FU Polish Ministry of Science and Higher Education [N/N203/402739]; NASA Astrobiology Institute under Institute for Astronomy, University of Hawaii [NNA09DA77A]; NASA EXOB [NNX09AN05G]; KASI [2012-1-410-02]; Department of Culture, Arts and Leisure (DCAL); Korea Astronomy and Space Science Institute (KASI) under the KRCF (Korea Research Council of Fundamental Science and Technology) FX Research by T. C. H. is carried out at the Korea Astronomy and Space Science Institute (KASI) under the KRCF (Korea Research Council of Fundamental Science and Technology) Young Scientist Research Fellowship Program. Numerical simulations were carried out on the "Beehive" Computing Cluster at Armagh Observatory (UK). T. C. H. acknowledges Martin Murphy for assistance in using the Beehive computing cluster and Professor Chun-Hwey Kim (Chungbuk National University, Cheongju, South Korea) for stimulating discussions on eclipsing binaries and their period variations. K. G. is supported by the Polish Ministry of Science and Higher Education through grant N/N203/402739. N.H. acknowledges support from NASA Astrobiology Institute under Cooperative Agreement NNA09DA77A at the Institute for Astronomy, University of Hawaii, and NASA EXOB grant NNX09AN05G. J.W.L., C. U. L., and T. C. H. acknowledges support from KASI registered under grant number 2012-1-410-02. Astronomical research at Armagh Observatory is funded by the Department of Culture, Arts and Leisure (DCAL). NR 36 TC 14 Z9 14 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 AUG PY 2012 VL 144 IS 2 AR 34 DI 10.1088/0004-6256/144/2/34 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600005 ER PT J AU Jarrett, TH Masci, F Tsai, CW Petty, S Cluver, M Assef, RJ Benford, D Blain, A Bridge, C Donoso, E Eisenhardt, P Fowler, J Koribalski, B Lake, S Neill, JD Seibert, M Sheth, K Stanford, S Wright, E AF Jarrett, T. H. Masci, F. Tsai, C. W. Petty, S. Cluver, M. Assef, Roberto J. Benford, D. Blain, A. Bridge, C. Donoso, E. Eisenhardt, P. Fowler, J. Koribalski, B. Lake, S. Neill, James D. Seibert, M. Sheth, K. Stanford, S. Wright, E. TI CONSTRUCTING A WISE HIGH RESOLUTION GALAXY ATLAS SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: fundamental parameters; galaxies: statistics; infrared: galaxies; surveys; techniques: image processing ID ON-ORBIT PERFORMANCE; EVOLUTION-EXPLORER; MISSION AB After eight months of continuous observations, the Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at 3.4 mu m, 4.6 mu m, 12 mu m, and 22 mu m. We have begun a dedicated WISE High Resolution Galaxy Atlas project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we summarize the deconvolution techniques used to significantly improve the spatial resolution of WISE imaging, specifically designed to study the internal anatomy of nearby galaxies. As a case study, we present results for the galaxy NGC 1566, comparing the WISE enhanced-resolution image processing to that of Spitzer, Galaxy Evolution Explorer, and ground-based imaging. This is the first paper in a two-part series; results for a larger sample of nearby galaxies are presented in the second paper. C1 [Jarrett, T. H.; Donoso, E.] CALTECH, IPAC, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Petty, S.; Lake, S.; Wright, E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Cluver, M.] Australian Astron Observ, Epping, NSW 1710, Australia. [Assef, Roberto J.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Benford, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blain, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bridge, C.; Neill, James D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Koribalski, B.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia. [Seibert, M.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Assef, Roberto J.; Sheth, K.] NASA, Postdoctoral Program, NRAO, Charlottesville, VA 22903 USA. [Stanford, S.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. RP Jarrett, TH (reprint author), CALTECH, IPAC, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM jarrett@ipac.caltech.edu RI Benford, Dominic/D-4760-2012; OI Benford, Dominic/0000-0002-9884-4206; Cluver, Michelle/0000-0002-9871-6490 FU NASA; NASA Postdoctoral Program at the Jet Propulsion Laboratory; National Aeronautics and Space Administration FX This work is based (in part) on observations made with the Spitzer and research using the NASA/IPAC Extragalactic Database (NED) and IPAC Infrared Science Archive, all are operated by JPL, Caltech, under a contract with the National Aeronautics and Space Administration. Support for this work was provided by NASA through an award issued by JPL/Caltech. R.J.A. 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 publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 16 TC 24 Z9 24 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2012 VL 144 IS 2 AR 68 DI 10.1088/0004-6256/144/2/68 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600039 ER PT J AU Kastner, JH Montez, R Balick, B Frew, DJ Miszalski, B Sahai, R Blackman, E Chu, YH De Marco, O Frank, A Guerrero, MA Lopez, JA Rapson, V Zijlstra, A Behar, E Bujarrabal, V Corradi, RLM Nordhaus, J Parker, QA Sandin, C Schonberner, D Soker, N Sokoloski, JL Steffen, M Ueta, T Villaver, E AF Kastner, J. H. Montez, R., Jr. Balick, B. Frew, D. J. Miszalski, B. Sahai, R. Blackman, E. Chu, Y. -H. De Marco, O. Frank, A. Guerrero, M. A. Lopez, J. A. Rapson, V. Zijlstra, A. Behar, E. Bujarrabal, V. Corradi, R. L. M. Nordhaus, J. Parker, Q. A. Sandin, C. Schoenberner, D. Soker, N. Sokoloski, J. L. Steffen, M. Ueta, T. Villaver, E. TI THE CHANDRA X-RAY SURVEY OF PLANETARY NEBULAE (CHANPLANS): PROBING BINARITY, MAGNETIC FIELDS, AND WIND COLLISIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; planetary nebulae: general; stars: AGB and post-AGB ID GIANT-BRANCH STARS; ALL-SKY SURVEY; NUMERICAL SIMULATIONS; PREPLANETARY NEBULAE; BIPOLAR STRUCTURE; ACCRETION DISKS; LINE EMISSION; HELIX-NEBULA; HOT BUBBLE; LOW-MASS AB We present an overview of the initial results from the Chandra Planetary Nebula Survey (ChanPlaNS), the first systematic (volume-limited) Chandra X-Ray Observatory survey of planetary nebulae (PNe) in the solar neighborhood. The first phase of ChanPlaNS targeted 21 mostly high-excitation PNe within similar to 1.5 kpc of Earth, yielding four detections of diffuse X-ray emission and nine detections of X-ray-luminous point sources at the central stars (CSPNe) of these objects. Combining these results with those obtained from Chandra archival data for all (14) other PNe within similar to 1.5 kpc that have been observed to date, we find an overall X- ray detection rate of similar to 70% for the 35 sample objects. Roughly 50% of the PNe observed by Chandra harbor X-ray-luminous CSPNe, while soft, diffuse X-ray emission tracing shocks-in most cases, "hot bubbles"-formed by energetic wind collisions is detected in similar to 30%; five objects display both diffuse and point-like emission components. The presence (or absence) of X-ray sources appears correlated with PN density structure, in that molecule-poor, elliptical nebulae are more likely to display X-ray emission (either point-like or diffuse) than molecule-rich, bipolar, or Ring-like nebulae. All but one of the point-like CSPNe X-ray sources display X-ray spectra that are harder than expected from hot (similar to 100 kK) central stars emitting as simple blackbodies; the lone apparent exception is the central star of the Dumbbell nebula, NGC 6853. These hard X-ray excesses may suggest a high frequency of binary companions to CSPNe. Other potential explanations include self-shocking winds or PN mass fallback. Most PNe detected as diffuse X-ray sources are elliptical nebulae that display a nested shell/halo structure and bright ansae; the diffuse X-ray emission regions are confined within inner, sharp-rimmed shells. All sample PNe that display diffuse X-ray emission have inner shell dynamical ages less than or similar to 5 x 10(3) yr, placing firm constraints on the timescale for strong shocks due to wind interactions in PNe. The high-energy emission arising in such wind shocks may contribute to the high excitation states of certain archetypical "hot bubble" nebulae (e.g., NGC 2392, 3242, 6826, and 7009). C1 [Kastner, J. H.; Montez, R., Jr.; Rapson, V.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Kastner, J. H.; Montez, R., Jr.; Rapson, V.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Balick, B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Frew, D. J.; De Marco, O.; Parker, Q. A.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Frew, D. J.; De Marco, O.; Parker, Q. A.] Macquarie Univ, Macquarie Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia. [Miszalski, B.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Miszalski, B.] So African Large Telescope Fdn, ZA-7935 Observatory, South Africa. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Blackman, E.; Frank, A.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Chu, Y. -H.] Univ Illinois, Dept Astron, Champagne Urbana, IL USA. [Guerrero, M. A.] Inst Astrofis Astron, Granada 18008, Spain. [Lopez, J. A.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Zijlstra, A.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Behar, E.; Soker, N.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Bujarrabal, V.] Observ Astron Nacl, E-28803 Alcala De Henares, Spain. [Corradi, R. L. M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Corradi, R. L. M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Nordhaus, J.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA. [Parker, Q. A.] Australian Astron Observ, Epping, NSW 2121, Australia. [Sandin, C.; Schoenberner, D.; Steffen, M.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Ueta, T.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Villaver, E.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. RP Kastner, JH (reprint author), Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM jhk@cis.rit.edu; soker@physics.technion.ac.il; eva.villaver@uam.es RI Villaver, Eva/G-5710-2012; OI Villaver, Eva/0000-0003-4936-9418; Frew, David/0000-0002-3108-5284 FU Chandra X-ray Observatory Center [GO1-12025A]; NASA [NAS803060]; Spanish MEC [AYA2011-29754-C0302]; FEDER funds; U.S. Government Grant [NAG W-2166] FX This research was supported via award number GO1-12025A to RIT issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS803060. M.A.G. acknowledges partial support by grant AYA2011-29754-C0302 of the Spanish MEC (co-funded by FEDER funds). The Digitized Sky Surveys were produced at STScI under U.S. Government Grant NAG W-2166. NR 97 TC 34 Z9 34 U1 0 U2 4 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 AUG PY 2012 VL 144 IS 2 AR 58 DI 10.1088/0004-6256/144/2/58 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600029 ER PT J AU Krist, JE Stapelfeldt, KR Bryden, G Plavchan, P AF Krist, John E. Stapelfeldt, Karl R. Bryden, Geoffrey Plavchan, Peter TI HUBBLE SPACE TELESCOPE OBSERVATIONS OF THE HD 202628 DEBRIS DISK SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; stars: individual (HD 202628, HD 377, HD 7590, HD 38858, HD 45184, HD 73350, HD 135599, HD 145229, HD 187897, HD 201219) ID HR 8799; NEARBY STARS; K-DWARF; RING; PLANET; SEARCH; IMAGES; YOUNG; BELT; MASS AB A ring-shaped debris disk around the G2V star HD 202628 (d = 24.4 pc) was imaged in scattered light at visible wavelengths using the coronagraphic mode of the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. The ring is inclined by similar to 64 degrees from face-on, based on the apparent major/minor axis ratio, with the major axis aligned along P. A. = 130 degrees. It has inner and outer radii (>50% maximum surface brightness) of 139 AU and 193 AU in the northwest ansae and 161 AU and 223 AU in the southeast (Delta r/r approximate to 0.4). The maximum visible radial extent is similar to 254 AU. With mean surface brightness of V approximate to 24 mag arcsec(-2), this is the faintest debris disk observed to date in reflected light. The center of the ring appears offset from the star by similar to 28 AU (deprojected). An ellipse fit to the inner edge has an eccentricity of 0.18 and a = 158 AU. This offset, along with the relatively sharp inner edge of the ring, suggests the influence of a planetary-mass companion. There is a strong similarity with the debris ring around Fomalhaut, though HD 202628 is a more mature star with an estimated age of about 2 Gyr. We also provide surface brightness limits for nine other stars in our study with strong Spitzer excesses around which no debris disks were detected in scattered light (HD 377, HD 7590, HD 38858, HD 45184, HD 73350, HD 135599, HD 145229, HD 187897, and HD 201219). C1 [Krist, John E.; Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stapelfeldt, Karl R.] NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA. [Plavchan, Peter] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Krist, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NASA [NAS 5-26555, 1407, 12291] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. This work was funded by NASA via a Hubble Space Telescope General Observer Grant (program 12291) to the Jet Propulsion Laboratory, California Institute of Technology, and the Spitzer Project Science Office at JPL. NR 28 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2012 VL 144 IS 2 AR 45 DI 10.1088/0004-6256/144/2/45 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600016 ER PT J AU Nugent, CR Margot, JL Chesley, SR Vokrouhlicky, D AF Nugent, C. R. Margot, J. L. Chesley, S. R. Vokrouhlicky, D. TI DETECTION OF SEMIMAJOR AXIS DRIFTS IN 54 NEAR-EARTH ASTEROIDS: NEW MEASUREMENTS OF THE YARKOVSKY EFFECT SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; minor planets, asteroids: general; minor planets, asteroids: individual (1999 RQ36, Aten, Apollo, Ganymed, Geographos, Hathor, Icarus, Orpheus, Ra-Shalom); radiation mechanisms: thermal ID COMET; COLLISION; MAGNITUDE; STREAMS; MOTION AB We have identified and quantified semimajor axis drifts in near-Earth asteroids (NEAs) by performing orbital fits to optical and radar astrometry of all numbered NEAs. We focus on a subset of 54 NEAs that exhibit some of the most reliable and strongest drift rates. Our selection criteria include a Yarkovsky sensitivity metric that quantifies the detectability of semimajor axis drift in any given data set, a signal-to-noise metric, and orbital coverage requirements. In 42 cases, the observed drifts (similar to 10(-3) AU Myr(-1)) agree well with numerical estimates of Yarkovsky drifts. This agreement suggests that the Yarkovsky effect is the dominant non- gravitational process affecting these orbits, and allows us to derive constraints on asteroid physical properties. In 12 cases, the drifts exceed nominal Yarkovsky predictions, which could be due to inaccuracies in our knowledge of physical properties, faulty astrometry, or modeling errors. If these high rates cannot be ruled out by further observations or improvements in modeling, they would be indicative of the presence of an additional non-gravitational force, such as that resulting from a loss of mass of order a kilogram per second. We define the Yarkovsky efficiency f(Y) as the ratio of the change in orbital energy to incident solar radiation energy, and we find that typical Yarkovsky efficiencies are similar to 10-5. C1 [Nugent, C. R.; Margot, J. L.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Margot, J. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vokrouhlicky, D.] Charles Univ Prague, Inst Astron, CZ-18000 Prague 8, Czech Republic. RP Nugent, CR (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RI Margot, Jean-Luc/A-6154-2012 OI Margot, Jean-Luc/0000-0001-9798-1797 FU NSF Planetary Astronomy [AST-0929830, AST-1109772]; Czech Grant Agency [205/08/0064]; Research Program of the Czech Ministry of Education [MSM0021620860] FX C.N. and J.L.M. were partially funded by NSF Planetary Astronomy Grants AST-0929830 and AST-1109772. Part of this research was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. D.V. was partially supported by the Czech Grant Agency (grant 205/08/0064) and Research Program MSM0021620860 of the Czech Ministry of Education. NR 46 TC 20 Z9 20 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2012 VL 144 IS 2 AR 60 DI 10.1088/0004-6256/144/2/60 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600031 ER PT J AU Meneghini, R Liao, L Tanelli, S Durden, SL AF Meneghini, Robert Liao, Liang Tanelli, Simone Durden, Stephen L. TI Assessment of the Performance of a Dual-Frequency Surface Reference Technique Over Ocean SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Attenuation; precipitation; radar; surface scattering ID TRMM PRECIPITATION RADAR; PROFILING ALGORITHM; RAINFALL RETRIEVAL; WAVELENGTH RADAR; PATH ATTENUATION; CROSS-SECTIONS; MELTING LAYER; TOGA COARE; RETURNS AB The high correlation of the rain-free surface cross sections at two frequencies suggests that the estimate of differential path-integrated attenuation caused by precipitation along the radar beam can be obtained to a higher degree of accuracy than the path attenuation at either frequency. We explore this potential first analytically and then by examining data from the JPL dual-frequency airborne radar using measurements from the Tropical Composition, Cloud, and Climate Coupling experiment obtained during July-August 2007. Despite an improvement in the accuracy of the differential path attenuation, solving for parameters of the particle size distribution often requires not only this quantity but the single-wavelength path attenuation as well. We investigate a simple method of estimating the single-frequency path attenuation from the differential attenuation and compare this estimate with that derived directly from the surface return. C1 [Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Liao, Liang] Goddard Earth Sci Technol & Research Morgan State, Greenbelt, MD 20771 USA. [Tanelli, Simone; Durden, Stephen L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Meneghini, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM robert.meneghini-1@nasa.gov; liang.liao-1@nasa.gov; simone.tanelli@nasa.gov; steven.l.durden@nasa.gov FU NASA Headquarters under NASA's Precipitation Measurement Mission Grant [NNH06ZDA001N-PMM]; NASA FX Manuscript received March 31, 2011; revised September 2, 2011; accepted October 23, 2011. Date of publication February 3, 2012; date of current version July 18, 2012. This work was supported by Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement Mission Grant NNH06ZDA001N-PMM.; The authors wish to thank R. Rincon of NASA/GSFC for providing the measured drop size distributions and J. Jones of Wyle Information Systems for advice in processing the data. A portion of this research (Tanelli and Durden) was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 27 TC 10 Z9 10 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2012 VL 50 IS 8 BP 2968 EP 2977 DI 10.1109/TGRS.2011.2180727 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 977UV UT WOS:000306691200004 ER PT J AU Cavalieri, DJ Markus, T Ivanoff, A Miller, JA Brucker, L Sturm, M Maslanik, JA Heinrichs, JF Gasiewski, AJ Leuschen, C Krabill, W Sonntag, J AF Cavalieri, Donald J. Markus, Thorsten Ivanoff, Alvaro Miller, Jeff A. Brucker, Ludovic Sturm, Matthew Maslanik, James A. Heinrichs, John F. Gasiewski, Albin J. Leuschen, Carl Krabill, William Sonntag, John TI A Comparison of Snow Depth on Sea Ice Retrievals Using Airborne Altimeters and an AMSR-E Simulator SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Airborne altimetry; passive microwave remote sensing; sea ice; snow on sea ice ID MICROWAVE SIGNATURES; LASER ALTIMETRY; RADAR ALTIMETER; ROUGHNESS; ACCURACY; SYSTEM; SHEET AB A comparison of snow depths on sea ice was made using airborne altimeters and an Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E) simulator. The data were collected during the March 2006 National Aeronautics and Space Administration (NASA) Arctic field campaign utilizing the NASA P-3B aircraft. The campaign consisted of an initial series of coordinated surface and aircraft measurements over Elson Lagoon, Alaska and adjacent seas followed by a series of large-scale (100 km x 50 km) coordinated aircraft and AMSR-E snow depth measurements over portions of the Chukchi and Beaufort seas. This paper focuses on the latter part of the campaign. The P-3B aircraft carried the University of Colorado Polarimetric Scanning Radiometer (PSR-A), the NASA Wallops Airborne Topographic Mapper (ATM) lidar altimeter, and the University of Kansas Delay-Doppler (D2P) radar altimeter. The PSR-A was used as an AMSR-E simulator, whereas the ATM and D2P altimeters were used in combination to provide an independent estimate of snow depth. Results of a comparison between the altimeter-derived snow depths and the equivalent AMSR-E snow depths using PSR-A brightness temperatures calibrated relative to AMSR-E are presented. Data collected over a frozen coastal polynya were used to intercalibrate the ATM and D2P altimeters before estimating an altimeter snow depth. Results show that the mean difference between the PSR and altimeter snow depths is -2.4 cm (PSR minus altimeter) with a standard deviation of 7.7 cm. The RMS difference is 8.0 cm. The overall correlation between the two snow depth data sets is 0.59. C1 [Cavalieri, Donald J.; Markus, Thorsten; Ivanoff, Alvaro; Miller, Jeff A.; Brucker, Ludovic; Krabill, William; Sonntag, John] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Ivanoff, Alvaro] ADNET Syst Inc, Rockville, MD 20852 USA. [Miller, Jeff A.] Wyle Informat Sci, Mclean, VA 22102 USA. [Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD 21044 USA. [Sturm, Matthew] USA, Cold Reg Res & Engn Lab, Ft Wainwright, AK 99703 USA. [Maslanik, James A.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80262 USA. [Heinrichs, John F.] Ft Hays State Univ, Dept Geosci, Hays, KS 67601 USA. [Gasiewski, Albin J.] Univ Colorado, Dept Elect & Comp Engn, Boulder, CO 80309 USA. [Leuschen, Carl] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA. [Krabill, William] Sigma Space Inc, Wallops Isl, VA 23337 USA. [Sonntag, John] URS Corp, Wallops Isl, VA 23337 USA. RP Cavalieri, DJ (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM Donald.J.Cavalieri@nasa.gov; thorsten.markus@nasa.gov; Alvaro.Ivanoff@nasa.gov; jeff.miller@nasa.gov; ludovic.brucker@nasa.gov; matthew.sturm@usace.army.mil; james.maslanik@colorado.edu; jheinric@fhsu.edu; al.gasiewski@colorado.edu; leuschen@cresis.ku.edu; William.B.Krabill@nasa.gov; john.g.sonntag@nasa.gov RI Brucker, Ludovic/A-8029-2010 OI Brucker, Ludovic/0000-0001-7102-8084 FU NASA EOS Project Office; NASA; National Science Foundation FX The authors thank the NASA EOS Project Office and the NASA Cryospheric Sciences Program for their full support and the NASA P-3B pilots and their crew for meeting all flight objectives, all of which led to the successful completion of the Arctic 2006 field campaign. We also think the two anonymous reviewers whose comments and recommendations have resulted in a significantly improved manuscript.; The authors also acknowledge both the National Space Science and Technology Center in Huntsville, AL and the National Snow and Ice Data Center in Boulder, Colorado for processing and providing the AMSR-E snow depth on sea ice products. The ECMWF data used in this study are from the Research Data Archive (RDA) which is maintained by the Computational and Information Systems Laboratory at the National Center for Atmospheric Research which is sponsored by the National Science Foundation. The original data (data set number ds627.0) are available from the RDA (http://dss.ucar.edu). The AMSR-E sea ice drift gridded products were obtained from the Centre de Recherche et d'Exploitation Satellitaire (CERSAT), at IFREMER, Plouzane, France (http://cersat.ifremer.fr/data/discovery/by_product_type/gridded_product s). NR 22 TC 14 Z9 14 U1 0 U2 20 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 AUG PY 2012 VL 50 IS 8 BP 3027 EP 3040 DI 10.1109/TGRS.2011.2180535 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 977UV UT WOS:000306691200008 ER PT J AU Tselioudis, G Douvis, C Zerefos, C AF Tselioudis, George Douvis, Costas Zerefos, Christos TI Does dynamical downscaling introduce novel information in climate model simulations of precipitation change over a complex topography region? SO INTERNATIONAL JOURNAL OF CLIMATOLOGY LA English DT Article DE regional climate models; dynamical downscaling; added value; complex topography; precipitation change ID RESOLUTION AB Current climate and future climate-warming runs with the RegCM Regional Climate Model (RCM) at 50 and 11 km-resolutions forced by the ECHAM GCM are used to examine whether the increased resolution of the RCM introduces novel information in the precipitation field when the models are run for the mountainous region of the Hellenic peninsula. The model results are inter-compared with the resolution of the RCM output degraded to match that of the GCM, and it is found that in both the present and future climate runs the regional models produce more precipitation than the forcing GCM. At the same time, the RCM runs produce increases in precipitation with climate warming even though they are forced with a GCM that shows no precipitation change in the region. The additional precipitation is mostly concentrated over the mountain ranges, where orographic precipitation formation is expected to be a dominant mechanism. It is found that, when examined at the same resolution, the elevation heights of the GCM are lower than those of the averaged RCM in the areas of the main mountain ranges. It is also found that the majority of the difference in precipitation between the RCM and the GCM can be explained by their difference in topographic height. The study results indicate that, in complex topography regions, GCM predictions of precipitation change with climate warming may be dry biased due to the GCM smoothing of the regional topography. Copyright (c) 2011 Royal Meteorological Society C1 [Tselioudis, George; Douvis, Costas; Zerefos, Christos] Acad Athens, Ctr Atmospher Phys & Climatol, Athens 10672, Greece. [Tselioudis, George] Columbia Univ, NASA, GISS, New York, NY 10025 USA. RP Tselioudis, G (reprint author), Acad Athens, Ctr Atmospher Phys & Climatol, 24 Omirou Str, Athens 10672, Greece. EM gtselioudis@academyofathens.gr NR 12 TC 13 Z9 13 U1 0 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0899-8418 J9 INT J CLIMATOL JI Int. J. Climatol. PD AUG PY 2012 VL 32 IS 10 BP 1572 EP 1578 DI 10.1002/joc.2360 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 977KA UT WOS:000306656700011 ER PT J AU Jee, S Moser, RD AF Jee, SolKeun Moser, Robert D. TI Conservative integral form of the incompressible Navier-Stokes equations for a rapidly pitching airfoil SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Conservative form; Moving grid; Moving body; Pitching airfoil; Thrust ID FINITE-VOLUME METHOD; FLOW; SIMULATION; WAKE AB This study provides a simple moving-grid scheme which is based on a modified conservative form of the incompressible Navier-Stokes equations for flow around a moving rigid body. The modified integral form is conservative and seeks the solution of the absolute velocity. This approach is different from previous conservative differential forms [1-3] whose reference frame is not inertial. Keeping the reference frame being inertial results in simpler mathematical derivation to the governing equation which includes one dyadic product of velocity vectors in the convective term, whereas the previous [2,3] needs to obtain the time derivative with respect to non-inertial frames causing an additional dyadic product in the convective term. The scheme is implemented in a second-order accurate Navier-Stokes solver and maintains the order of the accuracy. After this verification, the scheme is validated for a pitching airfoil with very high frequencies. The simulation results match very well with the experimental results [4,5], including vorticity fields and a net thrust force. This airfoil simulation also provides detailed vortical structures near the trailing edge and time-evolving aerodynamic forces that are used to investigate the mechanism of the thrust force generation and the effects of the trailing edge shape. The developed moving-grid scheme demonstrates its validity for a rapid oscillating motion. (C) 2012 Elsevier Inc. All rights reserved. C1 [Jee, SolKeun] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Moser, Robert D.] Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA. [Moser, Robert D.] Univ Texas Austin, Inst Computat Engn & Sci, Austin, TX 78712 USA. RP Jee, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM solkeun.jee@nasa.gov FU Air Force Office of Scientific Research (AFOSR) [FA9550-05-1-0411]; Multidisciplinary University Research Initiative FX This work was supported by Air Force Office of Scientific Research (AFOSR Grant FA9550-05-1-0411) and Multidisciplinary University Research Initiative for the first author's graduate study at the University of Texas at Austin. Although this study was finished during the graduate study of the first author, the first author thanks the NASA Postdoctoral Program administrated by Oak Ridge Associated Universities for supports to write this paper up at the NASA Ames Research Center. The authors would like to thank Dr. Douglas Bohl and Dr. Manoochehr Koochesfahani for the discussion of their water-tunnel experimental data. The authors also would like to thank Dr. Murali Beddhu at Mississippi State University and Dr. Marcel Vinokur and Dr. Karim Shariff at the NASA Ames Research Center for valuable discussion about conservative forms of the Navier-Stokes equations. The authors wish to acknowledge Dr. Gianluca Iaccarino at Stanford University for providing CDPv2.3. NR 25 TC 1 Z9 1 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD AUG 1 PY 2012 VL 231 IS 19 BP 6268 EP 6289 DI 10.1016/j.jcp.2012.04.014 PG 22 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 976TC UT WOS:000306606900003 ER PT J AU MacKay, RA Gabb, TP Garg, A Rogers, RB Nathal, MV AF MacKay, R. A. Gabb, T. P. Garg, A. Rogers, R. B. Nathal, M. V. TI Influence of composition on microstructural parameters of single crystal nickel-base superalloys SO MATERIALS CHARACTERIZATION LA English DT Article DE Superalloy; Microstructure; Lattice mismatch; Phase chemistry; Turbine blade; Computational thermodynamic modeling ID NI-15CR-AL-TI-MO ALLOYS; MOLYBDENUM; BEHAVIOR; PHASE AB Fourteen nickel-base superalloy single crystals containing a range of chromium (Cr), cobalt (Co), molybdenum (Mo), and rhenium (Re) levels, and fixed amounts of aluminum (Al) and tantalum (Ta), were examined to determine the effect of bulk composition on basic microstructural parameters, including gamma' solvus, gamma' volume fraction, topologically close-packed (TCP) phases, gamma and gamma' phase chemistries, and gamma-gamma' lattice mismatch. Regression models describing the influence of bulk alloy composition on each of the microstructural parameters were developed and compared to predictions by a commercially-available software tool that used computational thermodynamics Co produced the largest change in gamma' solvus over the wide compositional range explored and Mo produced the biggest effect on the gamma lattice parameter over its range, although Re had a very potent influence on all naicrostructural parameters investigated. Changing the Cr, Co, Mo, and Re contents in the bulk alloy had an impact on their concentrations in they gamma matrix and to a smaller extent in the gamma' phase. The software tool under-predicted gamma' solvus temperatures and gamma' volume fractions, and over-predicted TCP phase volume fractions at 982 degrees C. However, the statistical regression models provided excellent estimations of the microstructural parameters and demonstrated the usefulness of such fummlas. (C) 2012 Elsevier Inc. All rights reserved. C1 [MacKay, R. A.; Gabb, T. P.; Garg, A.; Rogers, R. B.; Nathal, M. V.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Garg, A.] Univ Toledo, Toledo, OH 43606 USA. RP MacKay, RA (reprint author), NASA, Glenn Res Ctr, Mail Stop 49-1,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Rebecca.A.MacKay@nasa.gov FU NASA FX The authors wish to acknowledge Ms. A. Palczer of NASA Glenn Research Center for performing the DTA runs and Mr. D. Johnson of NASA Glenn Research Center for conducting phase extractions and ICP analyses. This work is supported by the Subsonic Fixed Wing project under NASA's Fundamental Aeronautics Program. NR 45 TC 10 Z9 12 U1 6 U2 35 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1044-5803 EI 1873-4189 J9 MATER CHARACT JI Mater. Charact. PD AUG PY 2012 VL 70 BP 83 EP 100 DI 10.1016/j.matchar.2012.05.001 PG 18 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Materials Science, Characterization & Testing SC Materials Science; Metallurgy & Metallurgical Engineering GA 978SL UT WOS:000306766000013 ER PT J AU Jain, R Yeo, H AF Jain, Rohit Yeo, Hyeonsoo TI Effects of torsion frequencies on rotor performance and structural loads with trailing edge flap SO SMART MATERIALS AND STRUCTURES LA English DT Article ID PREDICTION AB The effects of variation of blade torsion frequency on rotor performance and structural loads are investigated for a 1/rev active flap rotor and baseline rotor (no active control). The UH-60A four-bladed articulated main rotor is studied at a high-speed forward flight condition. The torsion frequencies are varied by modifying the spanwise torsional stiffness of the blade and/or the pitch link stiffness. First, a parametric/optimization study on the flap deployment schedule is carried out using lifting-line comprehensive analysis for the soft, baseline, and stiff rotor configurations, and then a higher fidelity coupled computational fluid dynamics-computational structural dynamics analysis is carried out for the optimal flap deployment. It is shown that with the soft rotor there is degradation in performance-of about 6% with respect to the baseline rotor in the case where the flaps are not activated, and of about 1% if flap deflections are applied. On the other hand, for the stiff rotor there is a slight improvement in performance-of about 2.3% when the flaps are not activated, and no appreciable change in the case where active flap deflections are applied. It appears that the peak performance achievable with using active flaps on a baseline stiffness rotor cannot be further improved significantly by varying the torsional frequencies. Variation of torsion frequency does not appear to have a significant influence on blade torsion moments and pitch link loads, although the 1/rev flap activation examined has an important role. C1 [Jain, Rohit; Yeo, Hyeonsoo] USA, Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA USA. RP Jain, R (reprint author), USA, Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA USA. EM rjain@merlin.arc.nasa.gov FU US Army Research, Development, and Engineering Command (AMRDEC) under SBIR [W911W6-08-C-0061] FX This work was presented at the Future Vertical Lift Aircraft Design Conference, San Francisco, California, January 18-20, 2012. This work was performed while the first author was an employee at HyPerComp Inc. and was sponsored by US Army Research, Development, and Engineering Command (AMRDEC) under SBIR Contract# W911W6-08-C-0061. Technical monitors are Drs Hyeonsoo Yeo and Mark Fulton at the US Army Aeroflightdynamics Directorate (AFDD). This is a work of the US Government and is not subject to copyright protection in the US. NR 27 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 J9 SMART MATER STRUCT JI Smart Mater. Struct. PD AUG PY 2012 VL 21 IS 8 AR 085026 DI 10.1088/0964-1726/21/8/085026 PG 11 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA 978BL UT WOS:000306713800027 ER PT J AU Breininger, DR Mazerolle, MJ Bolt, MR Legare, ML Drese, JH Hines, JE AF Breininger, D. R. Mazerolle, M. J. Bolt, M. R. Legare, M. L. Drese, J. H. Hines, J. E. TI Habitat fragmentation effects on annual survival of the federally protected eastern indigo snake SO ANIMAL CONSERVATION LA English DT Article DE detectability; encounter probability; survival; multistate model; endangered species ID DRYMARCHON-COUPERI; CAPTURE-RECAPTURE; TIMBER RATTLESNAKES; CENTRAL FLORIDA; ROAD MORTALITY; MARK-RECAPTURE; POPULATION; EXTINCTION; CONSERVATION; GEORGIA AB The eastern indigo snake (Drymarchon couperi) is a federally listed species, most recently threatened by habitat loss and habitat degradation. In an effort to estimate snake survival, a total of 103 individuals (59 males, 44 females) were followed using radio-tracking from January 1998 to March 2004 in three landscape types that had increasing levels of habitat fragmentation: (1) conservation cores; (2) conservation areas along highways; (3) suburbs. Because of a large number of radio-tracking locations underground for which the state of snakes (i.e. alive or dead) could not be assessed, we employed a multistate approach to model snake apparent survival and encounter probability of live and dead snakes. We predicted that male snakes in suburbs would have the lowest annual survival. We found a transmitter implantation effect on snake encounter probability, as snakes implanted on a given occasion had a lower encounter probability on the next visit compared with snakes not implanted on the previous occasion. Our results indicated that adult eastern indigo snakes have relatively high survival in conservation core areas, but greatly reduced survival in conservation areas along highways and in suburbs. These findings indicate that habitat fragmentation is likely to be the critical factor for species persistence. C1 [Breininger, D. R.; Bolt, M. R.; Drese, J. H.] NASA, Ecol Programs, Kennedy Space Ctr, FL 32899 USA. [Mazerolle, M. J.] Univ Quebec Abitibi Temiscamingue, Dept Appl Sci, Ctr Etud Foret, Rouyn Noranda, PQ, Canada. [Legare, M. L.] US Fish & Wildlife Serv, Merritt Isl Natl Wildlife Refuge, Titusville, FL USA. [Hines, J. E.] US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD USA. RP Breininger, DR (reprint author), NASA, Ecol Programs, IHA 300, Kennedy Space Ctr, FL 32899 USA. EM david.r.breninger@nasa.gov OI Mazerolle, Marc/0000-0002-0486-0310 FU Bailey Wildlife Foundation; National Aeronautics and Space Administration; US Air Force; US Geological Survey; Natural Sciences and Engineering Research Council of Canada FX The Bailey Wildlife Foundation, National Aeronautics and Space Administration, US Air Force, US Geological Survey, and Natural Sciences and Engineering Research Council of Canada funded this study. We thank G. Bailey, M. Bailey, J. Berish, P. Burger, C. Hall, R. Koester, L. LaClaire, P. Moler and R. Seigel. We also thank about 60 natural resource professionals that helped us capture indigo snakes for radio-tracking studies. J. D. Nichols provided constructive criticism on the manuscript and thoughtful advice on the modelling strategy. NR 61 TC 9 Z9 9 U1 12 U2 91 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD AUG PY 2012 VL 15 IS 4 BP 361 EP 368 DI 10.1111/j.1469-1795.2012.00524.x PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 975AV UT WOS:000306480000007 ER PT J AU Altamirano, D Strohmayer, T AF Altamirano, D. Strohmayer, T. TI LOW-FREQUENCY (11 mHz) OSCILLATIONS IN H1743-322: A NEW CLASS OF BLACK HOLE QUASI-PERIODIC OSCILLATIONS? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; black hole physics; stars: individual (H1743-322); X-rays: binaries ID RAY LIGHT CURVES; X-RAY; NEUTRON-STAR; TRANSIENT H1743-322; XTE J1550-564; GRS 1915+105; SPACED DATA; 4U 1608-52; OUTBURST; ACCRETION AB We report the discovery of quasi-periodic oscillations (QPOs) at similar to 11 mHz in two RXTE and one Chandra observations of the black hole candidate H1743-322. The QPO is observed only at the beginning of the 2010 and 2011 outbursts at similar hard color and intensity, suggestive of an accretion state dependence for the QPO. Although its frequency appears to be correlated with X-ray intensity on timescales of a day, in successive outbursts eight months apart, we measure a QPO frequency that differs by less than approximate to 2.2 mHz while the intensity had changed significantly. We show that this similar to 11 mHz QPO is different from the so-called Type C QPOs seen in black holes and that the mechanisms that produce the two flavors of variability are most probably independent. After comparing this QPO with other variability phenomena seen in accreting black holes and neutron stars, we conclude that it best resembles the so-called 1 Hz QPOs seen in dipping neutron star systems, although having a significantly lower (1-2 orders of magnitude) frequency. If confirmed, H1743-322 is the first black hole showing this type of variability. Given the unusual characteristics and the hard-state dependence of the similar to 11 mHz QPO, we also speculate whether these oscillations could instead be related to the radio jets observed in H1743-322. A systematic search for this type of low-frequency QPOs in similar systems is needed to test this speculation. In any case, it remains unexplained why these QPOs have only been seen in the last two outbursts of H1743-322. C1 [Altamirano, D.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Strohmayer, T.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Altamirano, D (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM d.altamirano@uva.nl NR 48 TC 10 Z9 10 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 AUG 1 PY 2012 VL 754 IS 2 AR L23 DI 10.1088/2041-8205/754/2/L23 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 975QY UT WOS:000306527200005 ER PT J AU Matt, SP MacGregor, KB Pinsonneault, MH Greene, TP AF Matt, Sean P. MacGregor, Keith B. Pinsonneault, Marc H. Greene, Thomas P. TI MAGNETIC BRAKING FORMULATION FOR SUN-LIKE STARS: DEPENDENCE ON DIPOLE FIELD STRENGTH AND ROTATION RATE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE magnetohydrodynamics (MHD); stars: magnetic field; stars: rotation; stars: solar-type; stars: winds, outflows ID SOLAR-TYPE STARS; POWERED STELLAR WINDS; ANGULAR-MOMENTUM LOSS; X-RAY-EMISSION; DYNAMICAL SIMULATIONS; LITHIUM DEPLETION; ACTIVITY CYCLE; EVOLUTION; MASS; PERIOD AB We use two-dimensional axisymmetric magnetohydrodynamic simulations to compute steady-state solutions for solar-like stellar winds from rotating stars with dipolar magnetic fields. Our parameter study includes 50 simulations covering a wide range of relative magnetic field strengths and rotation rates, extending from the slow-and approaching the fast-magnetic-rotator regimes. Using the simulations to compute the angular momentum loss, we derive a semi-analytic formulation for the external torque on the star that fits all of the simulations to a precision of a few percent. This formula provides a simple method for computing the magnetic braking of Sun-like stars due to magnetized stellar winds, which properly includes the dependence on the strength of the magnetic field, mass loss rate, stellar radius, surface gravity, and spin rate, and which is valid for both slow and fast rotators. C1 [Matt, Sean P.] CEA Irfu Univ Paris Diderot CNRS INSU, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [MacGregor, Keith B.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA. [Pinsonneault, Marc H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Greene, Thomas P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Matt, SP (reprint author), CEA Irfu Univ Paris Diderot CNRS INSU, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. EM sean.matt@cea.fr; kmac@ucar.edu; pinsonneault.1@osu.edu; thomas.p.greene@nasa.gov OI Matt, Sean/0000-0001-9590-2274 FU NASA Postdoctoral Program at Ames Research Center; ERC [207430 STARS2]; National Science Foundation; NASA's Origins of Solar Systems program [WBS 811073.02.07.01.89] FX S.P.M. was supported by the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA, and by the ERC through grant 207430 STARS2 (http://www.stars2.eu). The National Center for Atmospheric Research is sponsored by the National Science Foundation. T. P. G. acknowledges support from NASA's Origins of Solar Systems program via WBS 811073.02.07.01.89. NR 37 TC 55 Z9 55 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 AUG 1 PY 2012 VL 754 IS 2 AR L26 DI 10.1088/2041-8205/754/2/L26 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 975QY UT WOS:000306527200008 ER PT J AU Gabb, TP Webster, H Ribeiro, G Gorman, T Gayda, J AF Gabb, T. P. Webster, H. Ribeiro, G. Gorman, T. Gayda, J. TI Fatigue Life of Superalloy Haynes 188 in Hydrogen SO JOURNAL OF MATERIALS ENGINEERING AND PERFORMANCE LA English DT Article DE aerospace; environment; superalloys AB The effects of hydrogen and surface finish on the mean low cycle fatigue life of Haynes 188 were studied. Specimens were prepared and fatigue tested with gage sections having low stress ground (LSG) and electro-discharge machined (EDM) surfaces. Fatigue tests were performed at temperatures of 25 to 650 A degrees C with varied strain conditions, in hydrogen and helium environments. Fatigue life decreased with increasing strain range, strain ratio, temperature, and with hydrogen atmosphere. A Smith-Watson-Topper stress parameter could be used to account for variations in strain range and strain ratio, and most strongly influenced life. Hydrogen reduced fatigue life by about 5x (80%) at 25 A degrees C, but was much less harmful at 650 A degrees C. Standard EDM finish did not consistently reduce mean fatigue life from that of LSG finish specimens. Additional tests indicated fatigue life in hydrogen was maintained for varied EDM conditions, provided specimen roughness and maximum recast layer thickness were not excessive. C1 [Gabb, T. P.; Gayda, J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Webster, H.; Ribeiro, G.] ATK Missile Prod Grp, Palm Beach Gardens, FL 33410 USA. [Gorman, T.] Univ Dayton, Dayton, OH 45469 USA. RP Gabb, TP (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM tim.gabb@grc.nasa.gov FU NASA FX The authors wish to acknowledge the support of the NASA Hypersonics Program, Anthony Calomino and Diego Capriotti. Also acknowledged are Tina Malone, Brian Hastings, Michael Watwood, and Eric King, manager and engineers at NASA Marshall Space Flight Center overseeing the Hydrogen Fatigue Testing facility and fatigue testing machines. NR 8 TC 0 Z9 0 U1 3 U2 8 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1059-9495 J9 J MATER ENG PERFORM JI J. Mater. Eng. Perform. PD AUG PY 2012 VL 21 IS 8 BP 1687 EP 1695 DI 10.1007/s11665-011-0067-1 PG 9 WC Materials Science, Multidisciplinary SC Materials Science GA 975ZD UT WOS:000306549400013 ER PT J AU Han, JW Meyyappan, M Ahn, JH Choi, YK AF Han, Jin-Woo Meyyappan, M. Ahn, Jae-Hyuk Choi, Yang-Kyu TI Liquid gate dielectric field effect transistor for a radiation nose SO SENSORS AND ACTUATORS A-PHYSICAL LA English DT Article DE Field effect transistor; Liquid gate dielectric; Radiation sensor; Radiation nose ID SENSORS; DEVICES; SYSTEM AB Radiation sensors are essential to detect illicit radiological materials, nuclear waste management, radiochemistry, nuclear physics, and medical research. Detectors should be capable of uncovering various radiation sources with a good energy resolution and being adaptable to different platforms such as hand-held, desktop, and benchtop, which can be easily implemented for security check in harbors and airports. Many of the devices and systems presently in use are bulky and expensive. Herein, we present a new detection method and architecture based on metal oxide semiconductor field effect transistor. Some liquids react to radiation, leading to a change in properties such as dielectric constant. Inspired by such radiation-responsivity, we have constructed a transistor with a radiation-responsive liquid as a gate dielectric. Current-voltage characteristics of the device change upon gamma-ray irradiation. Different types of liquids that specifically interact with target radiations can be used in an array of transistors serving as a radiation nose in the future. Such a radiation nose can be adaptable to different platforms and for implementation as a dosimeter for radiotherapy patients, nuclear plant health and safety inspection, space travel, environmental monitoring, and sensors for security. Published by Elsevier B.V. C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ahn, Jae-Hyuk; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Dept Elect Engn, Taejon 305701, South Korea. RP Han, JW (reprint author), NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov FU Center Innovation Fund; National Research and Development Program [2010-0002108]; National Research Foundation of Korea; Korean government [2010-0018931] FX The work at NASA Ames was supported by a Center Innovation Fund and the authors thank John Hines for support of this work and discussion. The work in Korea was supported in part by the National Research and Development Program under Grant 2010-0002108 for the development of biomedical function monitoring biosensors and in part by the National Research Foundation of Korea funded by the Korean government under Grant 2010-0018931. NR 13 TC 0 Z9 0 U1 1 U2 6 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0924-4247 J9 SENSOR ACTUAT A-PHYS JI Sens. Actuator A-Phys. PD AUG PY 2012 VL 182 BP 1 EP 5 DI 10.1016/j.sna.2012.05.038 PG 5 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 976KQ UT WOS:000306583900001 ER PT J AU Kaufmann, P Holman, GD Su, Y de Castro, CGG Correia, E Fernandes, LOT de Souza, RV Marun, A Pereyra, P AF Kaufmann, Pierre Holman, Gordon D. Su, Yang Guillermo Gimenez de Castro, C. Correia, Emilia Fernandes, Luis O. T. de Souza, Rodney V. Marun, Adolfo Pereyra, Pablo TI Unusual Emissions at Various Energies Prior to the Impulsive Phase of the Large Solar Flare and Coronal Mass Ejection of 4 November 2003 SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections (CMEs); CME precursors; Solar flares; Sub-THz emissions; X-ray emissions ID CMES; MICROWAVE; BURSTS; PULSATIONS; INITIATION; RELEASE; REGIONS; MODELS AB The GOES X28 flare of 4 November 2003 was the largest ever recorded in its class. It produced the first evidence for two spectrally separated emission components, one at microwaves and the other in the THz range of frequencies. We analyzed the pre-flare phase of this large flare, twenty minutes before the onset of the major impulsive burst. This period is characterized by unusual activity in X-rays, sub-THz frequencies, H alpha, and microwaves. The CME onset occurred before the onset of the large burst by about 6 min. It was preceded by pulsations of 3 -aEuro parts per thousand 5 s periods at sub-THz frequencies together with X-ray and microwave enhancements. The sub-THz pulsations faded out as impulsive bursts were detected at 100 -aEuro parts per thousand 300 keV and 7 GHz, close to the time of the first H alpha brightening and the CME onset. The activities detected prior to and at the CME onset were located nearly 2 arcmin south of the following large flare, suggesting they were separate events. This unusual activity brings new clues to understanding the complex energy buildup mechanisms prior to the CME onset, occurring at a distinct location and well before the major flare that exploded afterwards. C1 [Kaufmann, Pierre; Guillermo Gimenez de Castro, C.; Correia, Emilia; Fernandes, Luis O. T.; de Souza, Rodney V.] Univ Presbiteriana Mackenzie, Escola Engn, CRAAM, BR-01302970 Sao Paulo, Brazil. [Kaufmann, Pierre] Univ Estadual Campinas, CCS, BR-13083970 Campinas, SP, Brazil. [Holman, Gordon D.; Su, Yang] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Su, Yang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Su, Yang] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Correia, Emilia] Inst Nacl Pesquisas Espaciais, BR-12201970 Sao Jose Dos Campos, SP, Brazil. [Marun, Adolfo; Pereyra, Pablo] Consejo Nacl Invest Cient & Tecn, San Juan, Argentina. RP Kaufmann, P (reprint author), Univ Presbiteriana Mackenzie, Escola Engn, CRAAM, BR-01302970 Sao Paulo, Brazil. EM kaufmann@craam.mackenzie.br RI Correia, Emilia/F-6802-2012; Su, Yang/J-5381-2014; Gimenez de Castro, Carlos Guillermo/I-4367-2016 OI Gimenez de Castro, Carlos Guillermo/0000-0002-8979-3582 FU RHESSI project; NASA Heliophysics Guest Investigator Grant; FAPESP; CNPq; Mackpesquisa; Argentina agency CONICET; US agency AFOSR FX We wish to thank an anonymous referee for very helpful comments. We acknowledge Dr. Dale Gary for providing the OVSA microwave burst spectrum. Gordon Holman and Yang Su acknowledge support from the RHESSI project and a NASA Heliophysics Guest Investigator Grant. This research was partially supported by the Brazilian agencies FAPESP, CNPq, Mackpesquisa, Argentina agency CONICET, and US agency AFOSR. NR 45 TC 2 Z9 2 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD AUG PY 2012 VL 279 IS 2 BP 465 EP 475 DI 10.1007/s11207-012-0040-7 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974MY UT WOS:000306440800009 ER PT J AU Lugaz, N Kintner, P Mostl, C Jian, LK Davis, CJ Farrugia, CJ AF Lugaz, N. Kintner, P. Moestl, C. Jian, L. K. Davis, C. J. Farrugia, C. J. TI Heliospheric Observations of STEREO-Directed Coronal Mass Ejections in 2008-2010: Lessons for Future Observations of Earth-Directed CMEs SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections; STEREO; Heliospheric imagers; Methods ID IN-SITU SIGNATURES; INNER HELIOSPHERE; PROPAGATION; KINEMATICS; SECCHI AB We present a study of coronal mass ejections (CMEs) which impacted one of the STEREO spacecraft between January 2008 and early 2010. We focus our study on 20 CMEs which were observed remotely by the Heliospheric Imagers (HIs) onboard the other STEREO spacecraft up to large heliocentric distances. We compare the predictions of the Fixed-I broken vertical bar and Harmonic Mean (HM) fitting methods, which only differ by the assumed geometry of the CME. It is possible to use these techniques to determine from remote-sensing observations the CME direction of propagation, arrival time and final speed which are compared to in-situ measurements. We find evidence that for large viewing angles, the HM fitting method predicts the CME direction better. However, this may be due to the fact that only wide CMEs can be successfully observed when the CME propagates more than 100(a similar to) from the observing spacecraft. Overall eight CMEs, originating from behind the limb as seen by one of the STEREO spacecraft can be tracked and their arrival time at the other STEREO spacecraft can be successfully predicted. This includes CMEs, such as the events on 4 December 2009 and 9 April 2010, which were viewed 130(a similar to) away from their direction of propagation. Therefore, we predict that some Earth-directed CMEs will be observed by the HIs until early 2013, when the separation between Earth and one of the STEREO spacecraft will be similar to the separation of the two STEREO spacecraft in 2009 -aEuro parts per thousand 2010. C1 [Lugaz, N.; Farrugia, C. J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Lugaz, N.; Kintner, P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kintner, P.] Univ Rochester, Rochester, NY 14627 USA. [Moestl, C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Moestl, C.] Graz Univ, Kanzelhohe Observ IGAM, Inst Phys, A-8010 Graz, Austria. [Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Jian, L. K.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA. [Davis, C. J.] SFTC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Davis, C. J.] Univ Reading, Dept Meteorol, Reading RG6 7BE, Berks, England. RP Lugaz, N (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM noe.lugaz@unh.edu; pkintner@u.rochester.edu; christian.moestl@ssl.berkeley.edu; lan.jian@nasa.gov; chris.davis@stfc.ac.uk; charlie.farrugia@unh.edu RI Lugaz, Noe/C-1284-2008; Scott, Christopher/H-8664-2012; Jian, Lan/B-4053-2010; OI Lugaz, Noe/0000-0002-1890-6156; Scott, Christopher/0000-0001-6411-5649; Jian, Lan/0000-0002-6849-5527; Moestl, Christian/0000-0001-6868-4152 FU NSF [AGS-0819653, AGS-1239699, AGS-1239704]; NASA [NNX-07AC13G, NNX-08AQ16G, NNX-12AB28G, NAS5-03131]; NSF; NASA; European Union [263252]; European Community [PIOF-GA-2010-272768] FX The authors would like to thank the anonymous referee for useful comments and suggestions, which helped improve the clarity of the manuscript. N.L. was supported during this work by NSF grants AGS-0819653, AGS-1239699 and AGS-1239704 and NASA grants NNX-07AC13G, NNX-08AQ16G and NNX-12AB28G. P. K. performed research for this work under a Research Experience for Undergraduates (REU) position at the University of Hawaii's Institute for Astronomy and funded by NSF. L.K.J.'s work was funded by NASA's SMD as part of the STEREO project, including the IMPACT investigation. This work was also partially supported by NASA STEREO program through grant NAS5-03131 to UC Berkeley and UNH and has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement 263252 [COMESEP]. C. M. was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme (PIOF-GA-2010-272768 [WILIS-CME]). SOHO and STEREO are projects of international cooperation between ESA and NASA. The SECCHI data are produced by an international consortium of Naval Research Laboratory, Lockheed Martin Solar and Astrophysics Lab, and NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory, and University of Birmingham (UK), Max-Planck-Institut fur Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee, and Institut d'Astrophysique Spatiale (France). NR 43 TC 11 Z9 11 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 AUG PY 2012 VL 279 IS 2 BP 497 EP 515 DI 10.1007/s11207-012-0007-8 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974MY UT WOS:000306440800011 ER PT J AU Savani, NP Davies, JA Davis, CJ Shiota, D Rouillard, AP Owens, MJ Kusano, K Bothmer, V Bamford, SP Lintott, CJ Smith, A AF Savani, N. P. Davies, J. A. Davis, C. J. Shiota, D. Rouillard, A. P. Owens, M. J. Kusano, K. Bothmer, V. Bamford, S. P. Lintott, C. J. Smith, A. TI Observational Tracking of the 2D Structure of Coronal Mass Ejections Between the Sun and 1 AU SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections (CMEs); Heliosphere; Solar-terrestrial relations; Solar wind ID IN-SITU OBSERVATIONS; SOLAR-WIND; INTERPLANETARY SCINTILLATION; MAGNETIC CLOUDS; HELIOSPHERIC IMAGERS; STEREO MISSION; SPACECRAFT; MORPHOLOGY; SIGNATURES; SECCHI AB The Solar TErrestrial RElations Observatory (STEREO) provides high cadence and high resolution images of the structure and morphology of coronal mass ejections (CMEs) in the inner heliosphere. CME directions and propagation speeds have often been estimated through the use of time-elongation maps obtained from the STEREO Heliospheric Imager (HI) data. Many of these CMEs have been identified by citizen scientists working within the SolarStormWatch project (www.solarstormwatch.com) as they work towards providing robust real-time identification of Earth-directed CMEs. The wide field of view of HI allows scientists to directly observe the two-dimensional (2D) structures, while the relative simplicity of time-elongation analysis means that it can be easily applied to many such events, thereby enabling a much deeper understanding of how CMEs evolve between the Sun and the Earth. For events with certain orientations, both the rear and front edges of the CME can be monitored at varying heliocentric distances (R) between the Sun and 1 AU. Here we take four example events with measurable position angle widths and identified by the citizen scientists. These events were chosen for the clarity of their structure within the HI cameras and their long track lengths in the time-elongation maps. We show a linear dependency with R for the growth of the radial width (W) and the 2D aspect ratio (.) of these CMEs, which are measured out to approximate to 0.7 AU. We estimated the radial width from a linear best fit for the average of the four CMEs. We obtained the relationships W = 0.14R + 0.04 for the width and chi = 2.5R + 0.86 for the aspect ratio (W and R in units of AU). C1 [Savani, N. P.] UCAR, Boulder, CO USA. [Savani, N. P.; Rouillard, A. P.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA. [Davies, J. A.; Davis, C. J.] STFC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Davis, C. J.; Owens, M. J.] Univ Reading, Space Environm Phys Grp, Reading RG6 6BB, Berks, England. [Shiota, D.] RIKEN, Computat Astrophys Lab, Adv Sci Inst, Wako, Saitama 3510198, Japan. [Rouillard, A. P.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Owens, M. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. [Kusano, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Kusano, K.] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan. [Bothmer, V.] Univ Gottingen, Inst Astrophys, Gottingen, Germany. [Bamford, S. P.] Univ Nottingham, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Lintott, C. J.; Smith, A.] Univ Oxford, Oxford OX1 3RH, England. RP Savani, NP (reprint author), UCAR, Boulder, CO USA. EM neel.savani02@imperial.ac.uk RI Owens, Mathew/B-3006-2010; Savani, Neel/G-4066-2014; Scott, Christopher/H-8664-2012; Bamford, Steven/E-8702-2010; OI Owens, Mathew/0000-0003-2061-2453; Savani, Neel/0000-0002-1916-7877; Scott, Christopher/0000-0001-6411-5649; Bamford, Steven/0000-0001-7821-7195; Shiota, Daikou/0000-0002-9032-8792; Smith, Arfon/0000-0002-3957-2474 FU JSPS London; NASA; Star Jack Eddy Postdoctoral Fellowship Program FX N.P.S. thanks the reviewer for his/her constructive comments and would also like to give my deepest appreciation to Japan Society for the Promotion of Science (JSPS) and JSPS London for the award of the (short-term) postdoctoral fellowship and the fantastic opportunity to work within Japan. 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. N.P.S. would like to thank N. Sheeley for useful discussion, and the science team and citizen scientists from the SolarStormWatch project and the Royal Observatory Greenwich. NR 68 TC 11 Z9 11 U1 2 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 AUG PY 2012 VL 279 IS 2 BP 517 EP 535 DI 10.1007/s11207-012-0041-6 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974MY UT WOS:000306440800012 ER PT J AU Dennis, BR Skinner, GK Li, MJ Shih, AY AF Dennis, B. R. Skinner, G. K. Li, M. J. Shih, A. Y. TI Very High-Resolution Solar X-Ray Imaging Using Diffractive Optics SO SOLAR PHYSICS LA English DT Article DE Imaging; Lenses; Solar flares; X-rays ID PHASE FRESNEL LENSES; ATOMIC DATABASE; EMISSION-LINES; ZONE PLATES; TELESCOPE; CHIANTI AB This paper describes the development of X-ray diffractive optics for imaging solar flares with better than 0.1 arcsec angular resolution. X-ray images with this resolution of the a parts per thousand yenaEuro parts per thousand 10 MK plasma in solar active regions and solar flares would allow the cross-sectional area of magnetic loops to be resolved and the coronal flare energy release region itself to be probed. The objective of this work is to obtain X-ray images in the iron-line complex at 6.7 keV observed during solar flares with an angular resolution as fine as 0.1 arcsec - over an order of magnitude finer than is now possible. This line emission is from highly ionized iron atoms, primarily Fe xxv, in the hottest flare plasma at temperatures in excess of a parts per thousand aEuro parts per thousand 10 MK. It provides information on the flare morphology, the iron abundance, and the distribution of the hot plasma. Studying how this plasma is heated to such high temperatures in such short times during solar flares is of critical importance in understanding these powerful transient events, one of the major objectives of solar physics. We describe the design, fabrication, and testing of phase zone plate X-ray lenses with focal lengths of a parts per thousand aEuro parts per thousand 100 m at these energies that would be capable of achieving these objectives. We show how such lenses could be included on a two-spacecraft formation-flying mission with the lenses on the spacecraft closest to the Sun and an X-ray imaging array on the second spacecraft in the focal plane a parts per thousand aEuro parts per thousand 100 m away. High-resolution X-ray images could be obtained when the two spacecraft are aligned with the region of interest on the Sun. Requirements and constraints for the control of the two spacecraft are discussed together with the overall feasibility of such a formation-flying mission. C1 [Dennis, B. R.; Skinner, G. K.; Li, M. J.; Shih, A. Y.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Skinner, G. K.] CRESST, College Pk, MD USA. [Skinner, G. K.] Univ Maryland, College Pk, MD 20742 USA. RP Dennis, BR (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. EM brian.r.dennis@nasa.gov; gerald.k.skinner@nasa.gov; mary.j.li@nasa.gov; albert.y.shih@nasa.gov FU Goddard Internal Research and Development (IRAD) program FX We thank John Krizmanic and Keith Gendreau for supporting the lens design and testing effort, Kenneth Phillips for providing the spectra shown in Figure 1 and for help with the solar objectives, and Amil Patel, Gang Hu, and Thitima Suwannasiri for their work fabricating the lenses in Goddard's Detector Development Lab. This project was supported with funding from the Goddard Internal Research and Development (IRAD) program. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA), and the University of Cambridge (UK). NR 22 TC 0 Z9 0 U1 4 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD AUG PY 2012 VL 279 IS 2 BP 573 EP 588 DI 10.1007/s11207-012-0016-7 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 974MY UT WOS:000306440800016 ER PT J AU Munasinghe, L Jun, T Rind, DH AF Munasinghe, Lalith Jun, Tackseung Rind, David H. TI Climate change: a new metric to measure changes in the frequency of extreme temperatures using record data SO CLIMATIC CHANGE LA English DT Article ID UNITED-STATES; MINIMUM TEMPERATURE; AIR-TEMPERATURE; DAILY MAXIMUM; DATA SET; TRENDS; PRECIPITATION; IMPACTS; CANADA; REGION AB Consensus on global warming is the result of multiple and varying lines of evidence, and one key ramification is the increase in frequency of extreme climate events including record high temperatures. Here we develop a metric-called "record equivalent draws" (RED)-based on record high (low) temperature observations, and show that changes in RED approximate changes in the likelihood of extreme high (low) temperatures. Since we also show that this metric is independent of the specifics of the underlying temperature distributions, RED estimates can be aggregated across different climates to provide a genuinely global assessment of climate change. Using data on monthly average temperatures across the global landmass we find that the frequency of extreme high temperatures increased 10-fold between the first three decades of the last century (1900-1929) and the most recent decade (1999-2008). A more disaggregated analysis shows that the increase in frequency of extreme high temperatures is greater in the tropics than in higher latitudes, a pattern that is not indicated by changes in mean temperature. Our RED estimates also suggest concurrent increases in the frequency of both extreme high and extreme low temperatures during 2002-2008, a period when we observe a plateauing of global mean temperature. Using daily extreme temperature observations, we find that the frequency of extreme high temperatures is greater in the daily minimum temperature time-series compared to the daily maximum temperature time-series. There is no such observable difference in the frequency of extreme low temperatures between the daily minimum and daily maximum. C1 [Jun, Tackseung] Kyung Hee Univ, Dept Econ, Seoul 130701, South Korea. [Munasinghe, Lalith] Columbia Univ Barnard Coll, Dept Econ, New York, NY 10027 USA. [Rind, David H.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Jun, T (reprint author), Kyung Hee Univ, Dept Econ, 1 Hoegi Dong, Seoul 130701, South Korea. EM tj32gm@gmail.com FU Kyung Hee University; Barnard College FX DelCCR2, HadCRUT3v, and ETCCDI data were provided by the Center for Climatic Research at the University of Delaware, Climate Research Unit at the University of East Anglia, and Expert Team on Climate Change Detection and Indices, respectively. We gratefully acknowledge financial support from the Kyung Hee University Research Grant (2009) and Barnard College Presidential Research Award (2010). The primary research was conducted while the second author was a Research Fellow at Barnard College, and on sabbatical leave from Kyung Hee University. He would like to thank both institutions for providing invaluable support to conduct research on climate change. We thank three anonymous referees for their constructive criticisms and many helpful suggestions. We also thank Cynthia Howells, Brendan O'Flaherty, Stephanie Pfirman, Sanjay Tikku, Moonkyoung Um, and Jerry Welch for encouragement and generous feedback on earlier versions of the paper. Finally, we thank Claire Fram and Britt Johnson for excellent research assistance. NR 60 TC 4 Z9 4 U1 0 U2 20 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 EI 1573-1480 J9 CLIMATIC CHANGE JI Clim. Change PD AUG PY 2012 VL 113 IS 3-4 BP 1001 EP 1024 DI 10.1007/s10584-011-0370-8 PG 24 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 973EA UT WOS:000306337100025 ER PT J AU Bozza, V Dominik, M Rattenbury, NJ Jorgensen, UG Tsapras, Y Bramich, DM Udalski, A Bond, IA Liebig, C Cassan, A Fouque, P Fukui, A Hundertmark, M Shin, IG Lee, SH Choi, JY Park, SY Gould, A Allan, A Mao, S Wyrzykowski, L Street, RA Buckley, D Nagayama, T Mathiasen, M Hinse, TC Novati, SC Harpsoe, K Mancini, L Scarpetta, G Anguita, T Burgdorf, MJ Horne, K Hornstrup, A Kains, N Kerins, E Kjaergaard, P Masi, G Rahvar, S Ricci, D Snodgrass, C Southworth, J Steele, IA Surdej, J Thone, CC Wambsganss, J Zub, M Albrow, MD Batista, V Beaulieu, JP Bennett, DP Caldwell, JAR Cole, AA Cook, KH Coutures, C Dieters, S Prester, DD Donatowicz, J Greenhill, J Kane, SR Kubas, D Marquette, JB Martin, R Menzies, J Pollard, KR Sahu, KC Williams, A Szymanski, MK Kubiak, M Pietrzynski, G Soszynski, I Poleski, R Ulaczyk, K Depoy, DL Dong, S Han, C Janczak, J Lee, CU Pogge, RW Abe, F Furusawa, K Hearnshaw, JB Itow, Y Kilmartin, PM Korpela, AV Lin, W Ling, CH Masuda, K Matsubara, Y Miyake, N Muraki, Y Ohnishi, K Perrott, YC Saito, T Skuljan, L Sullivan, DJ Sumi, T Suzuki, D Sweatman, WL Tristram, PJ Wada, K Yock, PCM Gulbis, A Hashimoto, Y Kniazev, A Vaisanen, P AF Bozza, V. Dominik, M. Rattenbury, N. J. Jorgensen, U. G. Tsapras, Y. Bramich, D. M. Udalski, A. Bond, I. A. Liebig, C. Cassan, A. Fouque, P. Fukui, A. Hundertmark, M. Shin, I. -G. Lee, S. H. Choi, J. -Y. Park, S. -Y. Gould, A. Allan, A. Mao, S. Wyrzykowski, L. Street, R. A. Buckley, D. Nagayama, T. Mathiasen, M. Hinse, T. C. Novati, S. Calchi Harpsoe, K. Mancini, L. Scarpetta, G. Anguita, T. Burgdorf, M. J. Horne, K. Hornstrup, A. Kains, N. Kerins, E. Kjaergaard, P. Masi, G. Rahvar, S. Ricci, D. Snodgrass, C. Southworth, J. Steele, I. A. Surdej, J. Thoene, C. C. Wambsganss, J. Zub, M. Albrow, M. D. Batista, V. Beaulieu, J. -P. Bennett, D. P. Caldwell, J. A. R. Cole, A. A. Cook, K. H. Coutures, C. Dieters, S. Prester, D. Dominis Donatowicz, J. Greenhill, J. Kane, S. R. Kubas, D. Marquette, J. -B. Martin, R. Menzies, J. Pollard, K. R. Sahu, K. C. Williams, A. Szymanski, M. K. Kubiak, M. Pietrzynski, G. Soszynski, I. Poleski, R. Ulaczyk, K. DePoy, D. L. Dong, Subo Han, C. Janczak, J. Lee, C. -U. Pogge, R. W. Abe, F. Furusawa, K. Hearnshaw, J. B. Itow, Y. Kilmartin, P. M. Korpela, A. V. Lin, W. Ling, C. H. Masuda, K. Matsubara, Y. Miyake, N. Muraki, Y. Ohnishi, K. Perrott, Y. C. Saito, To Skuljan, L. Sullivan, D. J. Sumi, T. Suzuki, D. Sweatman, W. L. Tristram, P. J. Wada, K. Yock, P. C. M. Gulbis, A. Hashimoto, Y. Kniazev, A. Vaisanen, P. TI OGLE-2008-BLG-510: first automated real-time detection of a weak microlensing anomaly - brown dwarf or stellar binary? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: micro; planetary systems ID GRAVITATIONAL LENSING EXPERIMENT; FOLLOW-UP OBSERVATIONS; INITIAL MASS FUNCTION; GALACTIC BULGE; EXTRASOLAR PLANETS; OPTICAL DEPTH; LIGHT CURVES; EARTH MASS; EVENTS; SYSTEMS AB The microlensing event OGLE-2008-BLG-510 is characterized by an evident asymmetric shape of the peak, promptly detected by the Automated Robotic Terrestrial Exoplanet Microlensing Search (ARTEMiS) system in real time. The skewness of the light curve appears to be compatible both with binary-lens and binary-source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly and our analysis demonstrate that: (1) automated real-time detection of weak microlensing anomalies with immediate feedback is feasible, efficient and sensitive, (2) rather common weak features intrinsically come with ambiguities that are not easily resolved from photometric light curves, (3) a modelling approach that finds all features of parameter space rather than just the favourite model is required and (4) the data quality is most crucial, where systematics can be confused with real features, in particular small higher order effects such as orbital motion signatures. It moreover becomes apparent that events with weak signatures are a silver mine for statistical studies, although not easy to exploit. Clues about the apparent paucity of both brown-dwarf companions and binary-source microlensing events might hide here. C1 [Bozza, V.; Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy. [Bozza, V.] Sez Napoli, Grp Coll Salerno, INFN, Naples, Italy. [Dominik, M.; Liebig, C.; Hundertmark, M.; Kains, N.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Rattenbury, N. J.; Perrott, Y. C.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Jorgensen, U. G.; Mathiasen, M.; Hinse, T. C.; Harpsoe, K.; Kjaergaard, P.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Jorgensen, U. G.; Harpsoe, K.; Snodgrass, C.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Tsapras, Y.] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. [Tsapras, Y.] Univ London, Sch Math Sci, Astron Unit, London E1 4NS, England. [Bramich, D. M.; Kains, N.] ESO Headquarters, D-85748 Garching, Germany. [Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Soszynski, I.; Poleski, R.; Ulaczyk, K.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Bond, I. A.; Lin, W.; Ling, C. H.; Skuljan, L.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, Auckland 1330, New Zealand. [Liebig, C.; Cassan, A.; Wambsganss, J.; Zub, M.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Cassan, A.; Batista, V.; Beaulieu, J. -P.; Coutures, C.; Kubas, D.; Marquette, J. -B.] UPMC, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Fouque, P.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Shin, I. -G.; Lee, S. H.; Choi, J. -Y.; Park, S. -Y.; Han, C.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea. [Dong, Subo; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Allan, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Mao, S.; Kerins, E.] Univ Manchester, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Buckley, D.; Gulbis, A.; Kniazev, A.; Vaisanen, P.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Nagayama, T.] Nagoya Univ, Fac Sci, Dept Phys & Astrophys, Nagoya, Aichi 4648602, Japan. [Hinse, T. C.] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland. [Hinse, T. C.; Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Novati, S. Calchi] IIASS, Vietri Sul Mare, SA, Italy. [Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Anguita, T.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Ctr Astro Ingn, Santiago 306, Chile. [Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. [Burgdorf, M. J.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Hornstrup, A.] Danmarks Tekniske Univ, Inst Rumforskning Og Teknol, DK-2100 Kbenhavn, Denmark. [Masi, G.] Bellatrix Astron Observ, I-03023 Ceccano, FR, Italy. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran. [Rahvar, S.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Southworth, J.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Thoene, C. C.] Inst Astrofis Andalucia, E-18080 Granada, Spain. [Thoene, C. C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Snodgrass, C.; Kubas, D.] ESO, Santiago 19001 19, Chile. [Albrow, M. D.; Bennett, D. P.; Pollard, K. R.; Hearnshaw, J. B.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Caldwell, J. A. R.] McDonald Observ, Fort Davis, TX 79734 USA. [Thoene, C. C.; Cole, A. A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Cook, K. H.] Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94551 USA. [Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia. [Donatowicz, J.] Vienna Univ Technol, A-1040 Vienna, Austria. [Kane, S. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia. [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Dong, Subo] Inst Adv Study, Princeton, NJ 08540 USA. [Janczak, J.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Abe, F.; Furusawa, K.; Itow, Y.; Masuda, K.; Matsubara, Y.; Miyake, N.; Sumi, T.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Kilmartin, P. M.; Tristram, P. J.] Mt John Observ, Lake Tekapo 8770, New Zealand. [Korpela, A. V.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Hashimoto, Y.] Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 11677, Taiwan. RP Bozza, V (reprint author), Univ Salerno, Dipartimento Fis ER Caianiello, Via Ponte Don Melillo, I-84084 Fisciano, SA, Italy. EM md35@st-andrews.ac.uk RI Dong, Subo/J-7319-2012; Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013; Williams, Andrew/K-2931-2013; Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; OI Snodgrass, Colin/0000-0001-9328-2905; Williams, Andrew/0000-0001-9080-0105; Hundertmark, Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855; Thone, Christina/0000-0002-7978-7648; Ricci, Davide/0000-0002-9790-0552 FU Danish Natural Science Foundation (FNU); Danish National Research Foundation; National Research Foundation of Korea [2009-0081561]; NSF [AST-0757888]; NASA [NNX08AF40G]; NASA through the Sagan Fellowship Program; International Institute for Advanced Scientific Studies; German Research Foundation (DFG); KRCF Young Scientist Research Fellowship Programme; Korea Astronomy and Space Science Institute (KASI) [2012-1-410-02]; Communaute francaise de Belgique - Actions de recherche concertees - Academie universitaire Wallonie-Europe; European Research Council under the European Community [246678]; Mt Canopus Observatory; Qatar National Research Fund (QNRF) [NPRP 09-476-1-078]; California Institute of Technology (Caltech); [JSPS20340052]; [JSPS20740104]; [MEXT19015005] FX The Danish 1.54 m telescope is operated based on a grant from the Danish Natural Science Foundation (FNU). The 'Dark Cosmology Centre' is funded by the Danish National Research Foundation. Work by C. Han was supported by a grant of National Research Foundation of Korea (2009-0081561). Work by AG was supported by NSF grant AST-0757888. Work by BSG, AG and RWP was supported by NASA grant NNX08AF40G. Work by SD was performed under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. The MOA team acknowledges support by grants JSPS20340052, JSPS20740104 and MEXT19015005. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT). LM acknowledges support for this work by research funds of the International Institute for Advanced Scientific Studies. MH acknowledges support by the German Research Foundation (DFG). TCH is funded through the KRCF Young Scientist Research Fellowship Programme. CUL acknowledges support by Korea Astronomy and Space Science Institute (KASI) grant 2012-1-410-02. DR (boursier FRIA) and JSurdej acknowledge support from the Communaute francaise de Belgique - Actions de recherche concertees - Academie universitaire Wallonie-Europe. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement no. 246678. Dr David Warren provided support for the Mt Canopus Observatory. MD, YT, DMB, CL, MH, RAS, KH and CS are thankful to Qatar National Research Fund (QNRF), member of Qatar Foundation, for support by grant NPRP 09-476-1-078. NR 74 TC 8 Z9 8 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 AUG PY 2012 VL 424 IS 2 BP 902 EP 918 DI 10.1111/j.1365-2966.2012.21233.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800008 ER PT J AU Balona, LA Breger, M Catanzaro, G Cunha, MS Handler, G Kolaczkowski, Z Kurtz, DW Murphy, S Niemczura, E Paparo, M Smalley, B Szabo, R Uytterhoeven, K Christiansen, JL Uddin, K Stumpe, MC AF Balona, L. A. Breger, M. Catanzaro, G. Cunha, M. S. Handler, G. Kolaczkowski, Z. Kurtz, D. W. Murphy, S. Niemczura, E. Paparo, M. Smalley, B. Szabo, R. Uytterhoeven, K. Christiansen, J. L. Uddin, K. Stumpe, M. C. TI Unusual high-frequency oscillations in the Kepler delta Scuti star KIC 4840675 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; binaries: spectroscopic; stars: individual: KIC 4840675; stars: oscillations; stars: variables: d Scuti ID SOLAR-LIKE OSCILLATIONS; A-TYPE STARS; INITIAL CHARACTERISTICS; EFFECTIVE TEMPERATURES; AMPLITUDE VARIABILITY; PULSATING STARS; INPUT CATALOG; CADENCE DATA; RED GIANTS; CONVECTION AB We show that the star KIC 4840675 observed by Kepler is composed of three stars with a rapidly rotating A-type star and two solar-type fainter companions. The A-type star is a d Scuti variable with a dominant mode and many other modes of lower amplitude, including several low-frequency variations. The low-frequency variation with highest amplitude can be interpreted as rotational modulation with the light curve changing with time. However, the most interesting aspect of this star is a triplet of independent modes in the range 118129 d-1 (1.41.5 mHz), which is far outside the range of typical d Scuti frequencies. We discuss the possibility that these modes could be solar-like oscillations, oscillations of the roAp type or due to an unseen pulsating compact companion. C1 [Balona, L. A.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Breger, M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Catanzaro, G.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Cunha, M. S.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Cunha, M. S.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal. [Handler, G.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Kolaczkowski, Z.; Niemczura, E.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Kurtz, D. W.; Murphy, S.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Paparo, M.; Szabo, R.] Konkoly Observ MTA CSFK, H-1121 Budapest, Hungary. [Smalley, B.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Uytterhoeven, K.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Uytterhoeven, K.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Christiansen, J. L.; Stumpe, M. C.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Uddin, K.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Balona, LA (reprint author), S African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa. EM lab@saao.ac.za OI Murphy, Simon/0000-0002-5648-3107 FU NASA's Science Mission Directorate; National Research Foundation; Hungarian OTKA [K83790, MB08C 81013]; 'Lendulet' programme; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P 21830-N16 (MB)]; Ciencia; FCT (Portugal); POPH/FSE (EC); Spanish National Plan of RD; [PTDC/CTEAST/098754/2008]; [AYA2010-17803] FX The authors wish to thank the Kepler team for their generosity in allowing the data to be released to the Kepler Asteroseismic Science Consortium (KASC) ahead of public release and for their outstanding efforts which have made these results possible. Funding for the Kepler mission is provided by NASA's Science Mission Directorate.; LAB wishes to express his sincere thanks to the South African Astronomical Observatory and the National Research Foundation for financial support. RS has been supported by the Hungarian OTKA grants K83790 and MB08C 81013, the 'Lendulet' programme and the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. This investigation has been supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung through project P 21830-N16 (MB). MSC is supported by a Ciencia 2007 contract and the project PTDC/CTEAST/098754/2008, funded by FCT (Portugal) and POPH/FSE (EC). KU acknowledges financial support by the Spanish National Plan of R&D for 2010, project AYA2010-17803. We thank the Spanish Night-Time Allocation Committee (CAT) for awarding time to the proposal 61-NOT7/10A. NR 44 TC 7 Z9 7 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2012 VL 424 IS 2 BP 1187 EP 1196 DI 10.1111/j.1365-2966.2012.21295.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800028 ER PT J AU Wyatt, MC Kennedy, G Sibthorpe, B Moro-Martin, A Lestrade, JF Ivison, RJ Matthews, B Udry, S Greaves, JS Kalas, P Lawler, S Su, KYL Rieke, GH Booth, M Bryden, G Horner, J Kavelaars, JJ Wilner, D AF Wyatt, M. C. Kennedy, G. Sibthorpe, B. Moro-Martin, A. Lestrade, J. -F. Ivison, R. J. Matthews, B. Udry, S. Greaves, J. S. Kalas, P. Lawler, S. Su, K. Y. L. Rieke, G. H. Booth, M. Bryden, G. Horner, J. Kavelaars, J. J. Wilner, D. TI Herschel imaging of 61 Vir: implications for the prevalence of debris in low-mass planetary systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: formation; planet-disc interactions; circumstellar matter; planetary systems ID SOLAR-TYPE STARS; SUN-LIKE STARS; STEADY-STATE EVOLUTION; TERRESTRIAL PLANETS; GIANT PLANETS; NEARBY STARS; SUPER-EARTHS; HOT DUST; HD 69830; DISKS AB This paper describes Herschel observations of the nearby (8.5 pc) G5V multi-exoplanet host star 61 Vir at 70, 100, 160, 250, 350 and 500 m carried out as part of the DEBRIS survey. These observations reveal emission that is significantly extended out to a distance of >15 arcsec with a morphology that can be fitted by a nearly edge-on (77 degrees inclination) radially broad (from 30 au out to at least 100 au) debris disc of fractional luminosity 2.7 x 10(-5), with two additional (presumably unrelated) sources nearby that become more prominent at longer wavelengths. Chance alignment with a background object seen at 1.4 GHz provides potential for confusion, however, the stars 1.4 arcsec yr-1 proper motion allows archival Spitzer 70 m images to confirm that what we are interpreting as disc emission really is circumstellar. Although the exact shape of the discs inner edge is not well constrained, the region inside 30 au must be significantly depleted in planetesimals. This is readily explained if there are additional planets outside those already known (i.e. in the 0.530 au region), but is also consistent with collisional erosion. We also find tentative evidence that the presence of detectable debris around nearby stars correlates with the presence of the lowest mass planets that are detectable in current radial velocity surveys. Out of an unbiased sample of the nearest 60 G stars, 11 are known to have planets, of which six (including 61 Vir) have planets that are all less massive than Saturn, and four of these have evidence for debris. The debris towards one of these planet hosts (HD 20794) is reported here for the first time. This fraction (4/6) is higher than that expected for nearby field stars (15 per cent), and implies that systems that form low-mass planets are also able to retain bright debris discs. We suggest that this correlation could arise because such planetary systems are dynamically stable and include regions that are populated with planetesimals in the formation process where the planetesimals can remain unperturbed over Gyr time-scales. C1 [Wyatt, M. C.; Kennedy, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sibthorpe, B.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Moro-Martin, A.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain. [Lestrade, J. -F.] Observ Paris, F-75014 Paris, France. [Matthews, B.; Booth, M.; Kavelaars, J. J.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Udry, S.] Observ Univ Geneve, CH-1290 Versoix, Switzerland. [Greaves, J. S.] Univ St Andrews, Scottish Univ Phys Alliance, St Andrews KY16 9SS, Fife, Scotland. [Kalas, P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kalas, P.] SETI Inst, Mountain View, CA 94043 USA. [Lawler, S.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Su, K. Y. L.; Rieke, G. H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Booth, M.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Horner, J.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wyatt, MC (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM wyatt@ast.cam.ac.uk RI Ivison, R./G-4450-2011; OI Ivison, R./0000-0001-5118-1313; Booth, Mark/0000-0001-8568-6336; Horner, Jonti/0000-0002-1160-7970; Su, Kate/0000-0002-3532-5580; Kennedy, Grant/0000-0001-6831-7547 FU European Union through ERC [279973] FX The authors are grateful to Ben Zuckerman for helpful comments on the paper. This work was supported by the European Union through ERC grant number no. 279973. NR 93 TC 52 Z9 52 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 AUG PY 2012 VL 424 IS 2 BP 1206 EP 1223 DI 10.1111/j.1365-2966.2012.21298.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800030 ER PT J AU Oates, SR Bayless, AJ Stritzinger, MD Prichard, T Prieto, JL Immler, S Brown, PJ Breeveld, AA De Pasquale, M Kuin, NPM Hamuy, M Holland, ST Taddia, F Roming, PWA AF Oates, S. R. Bayless, A. J. Stritzinger, M. D. Prichard, T. Prieto, J. L. Immler, S. Brown, P. J. Breeveld, A. A. De Pasquale, M. Kuin, N. P. M. Hamuy, M. Holland, S. T. Taddia, F. Roming, P. W. A. TI Multiwavelength observations of the Type IIb supernova 2009mg SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: individual: SN 2009mg ID ULTRA-VIOLET/OPTICAL TELESCOPE; X-RAY-EMISSION; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; IA SUPERNOVAE; LIGHT CURVES; IB SUPERNOVAE; MASS-LOSS; SN 1993J; PRESUPERNOVA EVOLUTION; ABSOLUTE MAGNITUDES AB We present Swift Ultra-Violet Optical Telescope and X-Ray Telescope (XRT) observations, and visual wavelength spectroscopy of the Type IIb supernova (SN) 2009mg, discovered in the Sb galaxy ESO 121-G26. The observational properties of SN 2009mg are compared to the prototype Type IIb SNe 1993J and 2008ax, with which we find many similarities. However, minor differences are discernible including SN 2009mg not exhibiting an initial fast decline or u-band upturn as observed in the comparison objects, and its rise to maximum is somewhat slower leading to slightly broader light curves. The late-time temporal index of SN 2009mg, determined from 40 d post-explosion, is consistent with the decay rate of SN 1993J, but inconsistent with the decay of 56Co. This suggests leakage of ?-rays out of the ejecta and a stellar mass on the small side of the mass distribution. Our XRT non-detection provides an upper limit on the mass-loss rate of the progenitor of . Modelling of the SN light curve indicates a kinetic energy of , an ejecta mass of and a 56Ni mass of 0.10 +/- 0.01 M?. C1 [Oates, S. R.; Breeveld, A. A.; Kuin, N. P. M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Bayless, A. J.; Prichard, T.; Roming, P. W. A.] SW Res Inst, Div 15, San Antonio, TX 78238 USA. [Stritzinger, M. D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Stritzinger, M. D.; Taddia, F.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Stritzinger, M. D.] Las Campanas Observ, Carnegie Observ, La Serena, Chile. [Prichard, T.; Roming, P. W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Prieto, J. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Immler, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Immler, S.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Immler, S.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol Code 668 8, Greenbelt, MD 20771 USA. [Brown, P. J.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [De Pasquale, M.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Hamuy, M.] Univ Chile, Dept Astron, Santiago, Chile. [Holland, S. T.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Oates, SR (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM sro@mssl.ucl.ac.uk RI Hamuy, Mario/G-7541-2016; OI stritzinger, maximilian/0000-0002-5571-1833 FU UK Space Agency; NASA [HF-51261.01-A]; STScI; AURA, Inc. for NASA [NAS 5-2655]; CONICYT through Centro de Astrofisica FONDAP [15010003]; Centro BASAL CATA [PFB 06]; Iniciativa Cientifica Milenio through the Millennium Center for Supernova Science [P10-064-F] FX We thank the referee for their useful comments. We also thank N. Morrell for performing spectroscopic observations. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) and the Leicester Database and Archive Service (LEDAS), provided by NASA's Goddard Space Flight Center and the Department of Physics and Astronomy, Leicester University, UK, respectively. SRO, AAB and NPMK acknowledge the support of the UK Space Agency. JLP acknowledges support from NASA through Hubble Fellowship Grant HF-51261.01-A awarded by STScI, which is operated by AURA, Inc. for NASA, under contract NAS 5-2655. MH acknowledges support by CONICYT through Centro de Astrofisica FONDAP 15010003, Centro BASAL CATA(PFB 06) and by Iniciativa Cientifica Milenio through the Millennium Center for Supernova Science (P10-064-F). NR 64 TC 4 Z9 4 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2012 VL 424 IS 2 BP 1297 EP 1306 DI 10.1111/j.1365-2966.2012.21311.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800038 ER PT J AU Wang, SS Guan, YP Li, ZJ Chao, Y Huang, JP AF Wang Shan-Shan Guan Yu-Ping Li Zhi-Jin Chao Yi Huang Jian-Ping TI Preliminary analyses on characteristics of sea surface temperatures in Kuroshio and its extension and relations to atmospheric circulations SO ACTA PHYSICA SINICA LA Chinese DT Article DE Kuroshio; sea surface temperature; Pacific decadal oscillation; El Nino-southern oscillation ID NORTH PACIFIC; VOLUME TRANSPORT; MESOSCALE EDDIES; VARIABILITY; OCEAN; MODE; SYSTEM; IMPACT; JAPAN; WATER AB A sea surface temperature (SST) based index, denoted as KI, is designed to characterize the holistic feature of Kuroshio east of the Tokara-kaikyo and its extension on the purpose of predict its SST trend. The KI is calculated on the base of the Hadley Center's monthly SSTs during the period 1941-2009. The wavelet analysis showed that the KI displays inter-annual and inter-decadal oscillations, dominated by quasi-triennial, quasi 7-yr and 20-yr time scales. In addition, the KI is shown to be phase-locking to seasonal cycles. It is found that there are significant temporally-lag correlations between the KI and the Pacific decadal oscillation (PDO) index as well as between the KI and the ENSO index. A set of composition analyses using the NCEP/NCAR reanalyses indicate that when the KI shows a positive anomaly, the SST becomes abnormally warm in the equatorial eastern. Pacific, the Hadley circulation is intensified, and consequently the transportation of the westerly momentum is enhanced. The enhanced Hadley circulation and transportation of the westerly momentum give rise to the deepened Aleutian low pressure, then cool the Kuroshio extension and the north Pacific basin and cause the KE extend east. The above "ENSO-PDO-Kuroshio" process need some response time, that is to say, we can forecast the SST variation on the Kuroshio on the basis of the ENSO and PDO, which is very significant to predict the climate in China. C1 [Wang Shan-Shan; Huang Jian-Ping] Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. [Guan Yu-Ping] Chinese Acad Sci, S China Sea Inst Oceanol, State Key Lab Trop Oceanog, Guangzhou 510301, Guangdong, Peoples R China. [Li Zhi-Jin; Chao Yi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wang, SS (reprint author), Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. EM guan@scsio.ac.cn RI Guan, Yuping /A-1119-2015 OI Guan, Yuping /0000-0003-2744-136X FU National Basic Research Program of China [2007CB411801]; JIFRESSE/UCLA, USA FX Project supported by the National Basic Research Program of China (Grant No. 2007CB411801) and the JIFRESSE/UCLA, USA. NR 49 TC 2 Z9 3 U1 0 U2 2 PU CHINESE PHYSICAL SOC PI BEIJING PA P O BOX 603, BEIJING 100080, PEOPLES R CHINA SN 1000-3290 J9 ACTA PHYS SIN-CH ED JI Acta Phys. Sin. PD AUG PY 2012 VL 61 IS 16 AR 169201 PG 11 WC Physics, Multidisciplinary SC Physics GA 010IX UT WOS:000309089200075 ER PT J AU McCraney, WT Farley, EV Kondzela, CM Naydenko, SV Starovoytov, AN Guyon, JR AF McCraney, W. Tyler Farley, Edward V. Kondzela, Christine M. Naydenko, Svetlana V. Starovoytov, Alexander N. Guyon, Jeffrey R. TI Genetic stock identification of overwintering chum salmon in the North Pacific Ocean SO ENVIRONMENTAL BIOLOGY OF FISHES LA English DT Article DE Chum salmon; Genetic stock identification; Migration; North Pacific Ocean ID ONCORHYNCHUS-KETA; RIM; MIGRATION AB Understanding stock and age-specific seasonal migrations of Pacific salmon during ocean residence is essential to both the conservation and management of this important resource. Based upon 11 microsatellites assayed on 265 individuals collected aboard international research surveys during winter 2009, we found substantial differences in the age-specific origin of chum salmon (Oncorhynchus keta) in the North Pacific Ocean. Overall, Asian stocks dominated the collections, however, ocean age 1 fish were primarily of Japanese origin and ocean age 2-3+ fish were predominantly of Russian origin. These results suggest that cohorts of chum salmon stocks migrate nonrandomly in the North Pacific Ocean and adjacent seas. C1 [McCraney, W. Tyler; Farley, Edward V.; Kondzela, Christine M.; Guyon, Jeffrey R.] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, NOAA, Juneau, AK 99801 USA. [Naydenko, Svetlana V.; Starovoytov, Alexander N.] TINRO Ctr, Pacific Res Fisheries Ctr, Vladivostok 690990, Russia. RP Guyon, JR (reprint author), Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, NOAA, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA. EM Jeff.Guyon@noaa.gov FU National Marine Fisheries Service; Bering Sea Fishermen's Association FX We thank the crew of the R/V TINRO for collecting the samples used in this study. Hanhvan Nguyen and Colby Marvin performed the DNA extractions, Sharon Wildes assisted with data scoring, and Adam Moles provided advice that greatly improved the manuscript. This work was funded by the National Marine Fisheries Service and the Bering Sea Fishermen's Association. The findings and conclusions in this paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service, NOAA. NR 15 TC 1 Z9 1 U1 1 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0378-1909 J9 ENVIRON BIOL FISH JI Environ. Biol. Fishes PD AUG PY 2012 VL 94 IS 4 BP 663 EP 668 DI 10.1007/s10641-011-9972-2 PG 6 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 971AM UT WOS:000306174000008 ER PT J AU Bristow, TF Kennedy, MJ Morrison, KD Mrofka, DD AF Bristow, Thomas F. Kennedy, Martin J. Morrison, Keith D. Mrofka, David D. TI The influence of authigenic clay formation on the mineralogy and stable isotopic record of lacustrine carbonates SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID GREEN RIVER FORMATION; WILKINS PEAK MEMBER; PARACHUTE CREEK MEMBER; CLOSED-BASIN LAKES; FORMATION EOCENE; UINTA BASIN; SALINE LAKE; DOLOMITE PRECIPITATION; OLDUVAI GORGE; DIAGENESIS AB The mineralogical, compositional and stable isotopic variability of lacustrine carbonates are frequently used as proxies for ancient paleoenvironmental change in continental settings, under the assumption that precipitated carbonates reflect conditions and chemistry of ancient lake waters. In some saline and alkaline lake systems, however, authigenic clay minerals, forming at or near the sediment water interface, are a major sedimentary component. Often these clays are rich in Mg, influencing the geochemical budget of lake waters, and are therefore expected to influence the properties of contemporaneous authigenic carbonate precipitates (which may also contain Mg). This paper documents evidence for a systematic feedback between clay mineral and carbonate authigenesis through multiple precessionally driven, m-scale sedimentary cycles in lacustrine oil-shale deposits of the Eocene Green River Formation from the Uinta Basin (NE Utah). In the studied section, authigenic, Mg-rich, trioctahedral smectite content varies cyclically between 9 and 39 wt.%. The highest concentrations occur in oil-shales and calcareous mudstones deposited during high lake level intervals that favored sedimentary condensation, lengthening the time available for clay diagenesis and reducing dilution by other siliciclastic phases. An inverse relation between dolomite percentage of carbonate and trioctahedral smectite abundance suggests the Mg uptake during clay authigenesis provides a first order control on carbonate mineralogy that better explains carbonate mineralogical trends than the possible alternative controls of (1) variable Mg/Ca ratios in lake water and (2) degree of microbial activity in sediments. We also observe that cyclical change in carbonate mineralogy, believed to be induced by clay authigenesis, also causes isotopic covariation between delta C-13(PDB) and delta O-18(PDB) of bulk sediments because of differences in the equilibrium fractionation factors of dolomite and calcite (similar to 2 parts per thousand and similar to 2.6%, respectively). This provides an alternative mechanism for the common pattern of isotopic covariation, which is typically attributed to the effect of simultaneous changes in water balance and biological activity on the carbon and oxygen isotopic composition of lake waters. These findings may help improve paleoenvironmental reconstructions based on lacustrine carbonate records by adding to the factors known to influence the mineralogical, compositional and stable isotopic signals recorded by lacustrine carbonates. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Bristow, Thomas F.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Kennedy, Martin J.] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. [Morrison, Keith D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Mrofka, David D.] Mt San Antonio Coll, Dept Earth Sci, Walnut, CA 91789 USA. RP Bristow, TF (reprint author), NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. EM thomas.f.bristow@nasa.gov FU NASA; O.K. Earl Fellowship; Blanchard Field Awards FX We thank C. Partin for field assistance, D. Pevear and R. Kleeberg for discussions and three anonymous reviewers for helpful comments. Research was supported by a NASA Postdoctoral Fellowship and the O.K. Earl Fellowship to T. F. B and Blanchard Field Awards to T.F.B and D.D.M. NR 77 TC 14 Z9 17 U1 2 U2 38 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG 1 PY 2012 VL 90 BP 64 EP 82 DI 10.1016/j.gca.2012.05.006 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 973DJ UT WOS:000306334200005 ER PT J AU Thompson, SA Sydeman, WJ Santora, JA Black, BA Suryan, RM Calambokidis, J Peterson, WT Bograd, SJ AF Thompson, Sarah Ann Sydeman, William J. Santora, Jarrod A. Black, Bryan A. Suryan, Robert M. Calambokidis, John Peterson, William T. Bograd, Steven J. TI Linking predators to seasonality of upwelling: Using food web indicators and path analysis to infer trophic connections SO PROGRESS IN OCEANOGRAPHY LA English DT Review ID CALIFORNIA CURRENT ECOSYSTEM; AUKLET PTYCHORAMPHUS-ALEUTICUS; CLIMATE-CHANGE; NORTHERN CALIFORNIA; CURRENT SYSTEM; REPRODUCTIVE-PERFORMANCE; PELAGIC ECOSYSTEM; COLONIAL SEABIRD; PREY CONSUMPTION; STABLE-ISOTOPES AB Upwelling in eastern boundary current systems is a primary driver of ecosystem productivity. Typically, peak upwelling occurs during spring and summer, but winter upwelling may also be important to ecosystem functions. In this study, we investigated the hypothesis that winter and spring/summer upwelling, operating through indirect trophic interactions, are important to a suite of top predators in the California Current. To test this hypothesis, we collated information on upwelling, chlorophyll-a concentrations, zooplankton and forage fish, and related these to predator responses including rockfish growth, salmon abundance, seabird productivity and phenology (timing of egg-laying), and whale abundance. Seabird diets served in part as food web indicators. We modeled pathways of response using path analysis and tested for significance of the dominant paths with multiple regression. We found support for the hypothesis that relationships between upwelling and top predator variables were mediated primarily by intermediate trophic levels. Both winter and summer upwelling were important in path models, as were intermediate lower and mid trophic level functional groups represented by chlorophyll-a, zooplankton, and forage fish. Significant pathways of response explained from 50% to 80% of the variation of seabird (Cassin's auklet (Ptychoramphus aleuticus) and common murre (Uria aalge)), humpback whale (Megaptera novaeangliae) and Chinook salmon (Oncorhynchus tshawytscha) dependent variables, whereas splitnose rockfish (Sebastes diploproa) showed no significant response pathways. Upwelling and trophic responses for salmon were established for both the year of ocean entry and the year of return, with zooplankton important in the year of ocean entry and forage fish important in the year of return. This study provides one of the first comparative investigations between upwelling and predators, from fish to marine mammals and birds within a geographically restricted area, demonstrates often difficult to establish "bottom-up" trophic interactions, and establishes the importance of seasonality of upwelling to various trophic connections and predator demographic traits. Understanding change in the seasonality of upwelling is therefore required to assess dynamics of commercially and recreationally important upper trophic level species in eastern boundary current ecosystems. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Thompson, Sarah Ann; Sydeman, William J.; Santora, Jarrod A.] Farallon Inst Adv Ecosyst Res, Petaluma, CA 94952 USA. [Black, Bryan A.; Suryan, Robert M.] Oregon State Univ, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. [Calambokidis, John] Cascadia Res, Olympia, WA 98501 USA. [Peterson, William T.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. [Bograd, Steven J.] NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Div Environm Res, Pacific Grove, CA 93950 USA. RP Thompson, SA (reprint author), Farallon Inst Adv Ecosyst Res, POB 750756, Petaluma, CA 94952 USA. EM sathompson@faralloninstitute.org RI Black, Bryan/A-7057-2009 FU NSF Grant [0929017]; NASA Grant [NNX09AU3NG]; California OPC/California Sea Grant [ENV-07]; USFWS and members and donors of PRBO (Farallon seabirds); NOAA-Fisheries (Stock Assessment Improvement Program, the Fisheries and the Environment Program, the US GLOBEC-Northeast Pacific Program (Peterson, Oregon copepods); California Department of Fish and Game; Sonoma County Water Agency (SCWA); Resources Law Group/Resources Legacy Fund Foundation FX This study was made possible by NSF Grant 0929017, NASA Grant NNX09AU3NG, and California OPC/California Sea Grant ENV-07. Field programs were supported by the USFWS and members and donors of PRBO (Farallon seabirds), NOAA-Fisheries (Stock Assessment Improvement Program, the Fisheries and the Environment Program, the US GLOBEC-Northeast Pacific Program (Peterson, Oregon copepods), the California Department of Fish and Game, and the Sonoma County Water Agency (SCWA). We thank PRBO Conservation Science for data contributions for this project. Analysis of remotely-sensed chlorophyll was facilitated by a grant from the Resources Law Group/Resources Legacy Fund Foundation. We thank Karina J. Nielsen for guidance on the use of path analysis and acknowledge Spencer Wood and the Sanak Island Food Web for feeding links. NR 87 TC 34 Z9 34 U1 8 U2 129 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0079-6611 J9 PROG OCEANOGR JI Prog. Oceanogr. PD AUG PY 2012 VL 101 IS 1 BP 106 EP 120 DI 10.1016/j.pocean.2012.02.001 PG 15 WC Oceanography SC Oceanography GA 960HT UT WOS:000305379300007 ER PT J AU Deau, E AF Deau, Estelle TI Variations of the apparent angular size of the Sun across the entire Solar System: Implications for planetary opposition surges SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Planetary surfaces; Phase curves; Opposition effect; Finite size of the Sun; Convolution; Deconvolution ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DISCRETE RANDOM-MEDIA; COHERENT BACKSCATTERING; SPHERICAL-PARTICLES; LIGHT-SCATTERING; PHASE CURVES; LABORATORY MEASUREMENTS; PARTICULATE SURFACES; WEAK-LOCALIZATION; REGOLITH ANALOGS AB We test several convolution and deconvolution models on phase curves at small phase angles (0.001 degrees < alpha < 1.5 degrees) that have the highest phase angle sampling to date. These curves were provided by cameras onboard several NASA missions (Clementine/UVVIS, Galileo/SSI and Cassini/ISS) when the Sun had different apparent angular radii (alpha(circle dot) = 0.266 degrees, 0.051 degrees, 0.028 degrees). For the smallest phase angles, the brightness of the objects (Moon, Europa and the Saturn's rings) exhibits a strong round-off below the angular size of the Sun. The brightness continues to increase below alpha(circle dot) before finally flattening at 0.4 alpha(circle dot). These behaviors are consistent with the convolution models tested. A simple deconvolution model is also used and agrees with laboratory measurements at extremely small phase angles that do not show any flattening [Psarev V. Ovcharenko A, Shkuratov YG, Belskaya I, Videen G. Photometry of particulate surfaces at extremely small phase angles. J Quant Spectrosc Radiat Transfer 2007;106:455-63]. Published by Elsevier Ltd. C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Deau, E (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM estelle.deau@jpl.nasa.gov FU NASA FX This study is performed at Jet Propulsion Laboratory (JPL), under contract with NASA and California Institute of Technology and is funded by the NASA Postdoctoral Program led by OakRidge Associated Universities (ORAU). NR 98 TC 5 Z9 5 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD AUG PY 2012 VL 113 IS 12 BP 1476 EP 1487 DI 10.1016/j.jqsrt.2012.02.040 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 961TZ UT WOS:000305493700008 ER PT J AU Kandula, M AF Kandula, Max TI Sound propagation in saturated gas-vapor-droplet suspensions considering the effect of transpiration on droplet evaporation SO APPLIED ACOUSTICS LA English DT Article DE Sound attenuation; Gas-vapor-droplets; Transpiration ID NONLINEAR PARTICLE RELAXATION; DILUTE SUSPENSIONS; NOISE-REDUCTION; WATER INJECTION; ATTENUATION; DISPERSION; WAVES; JET; FOG AB The sound attenuation and dispersion in saturated gas-vapor-droplet mixtures with evaporation has been investigated theoretically. The theory is based on an extension of the work of Davidson (1975) to accommodate the effects of transpiration on the linear particle relaxation processes of mass, momentum and energy transfer. It is shown that the inclusion of transpiration in the presence of mass transfer improves the agreement between the theory and the experimental data of Cole and Dobbins (1971) for sound attenuation in air-water fogs at low droplet mass concentrations. The results suggest that transpiration has an appreciable effect on both sound absorption and dispersion for both low and high droplet mass concentrations. (C) 2012 Elsevier Ltd. All rights reserved. C1 NASA, ESC Team QNA, Kennedy Space Ctr, FL 32899 USA. RP Kandula, M (reprint author), NASA, ESC Team QNA, Kennedy Space Ctr, FL 32899 USA. EM max.kandula-1@nasa.gov NR 24 TC 1 Z9 1 U1 1 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0003-682X J9 APPL ACOUST JI Appl. Acoust. PD AUG PY 2012 VL 73 IS 8 BP 849 EP 854 DI 10.1016/j.apacoust.2012.02.014 PG 6 WC Acoustics SC Acoustics GA 956RZ UT WOS:000305108100019 ER PT J AU Spencer, PD Hanselman, DH McKelvey, DR AF Spencer, Paul D. Hanselman, Dana H. McKelvey, Denise R. TI Simulation modeling of a trawl-acoustic survey design for patchily distributed species SO FISHERIES RESEARCH LA English DT Article DE Hydroacoustics; Double sampling; Trawl survey design; Patchiness; Spatial distributions ID ABUNDANCE; SEA; POPULATIONS AB Spatially patchy populations present challenges for precise estimation of abundance from surveys, which typically result in high estimation errors compared to surveys of more evenly distributed species. In this study, we used simulations to evaluate the performance of the Trawl and Acoustic Presence/Absence Survey design (TAPAS) in reducing the variability in estimated biomass. This approach is a double sampling design in which high-density patches observed in a first phase using hydroacoustics are subsequently more intensively sampled (relative to non-patch areas) in a second phase using trawls and area-swept methods. Information on Gulf of Alaska Pacific ocean perch (Sebastes alutus), a patchily distributed rock-fish species, was used to parameterize the simulations. The performance of the TAPAS design depends upon the degree to which high acoustic backscatter represents "patch" areas of high density and variability, as the relationship between backscatter and abundance of a given species can be affected by areas unavailable for sampling (i.e., the "dead zone") and the contribution of multiple species to the backscatter intensity. With a strong relationship between backscatter intensity and density, the TAPAS design resulted in improved precision compared to simple random sampling (SRS). Additionally, more intensive sampling of the patches occurred when areas of high backscatter intensity were randomly distributed over space rather than located in spatially correlated clusters. However, with a weak relationship between backscatter intensity and density, the precision of the TAPAS design was not substantially larger than SRS. The potential improvement in precision when a strong relationship exists between backscatter intensity and fish density offers motivation to continue to refine relationships between underlying fish density, acoustic backscatter, and trawl catches. Published by Elsevier B.V. C1 [Spencer, Paul D.; McKelvey, Denise R.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA. [Hanselman, Dana H.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. RP Spencer, PD (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, 7600 Sand Point Way NE, Seattle, WA 98115 USA. EM paul.spencer@noaa.gov FU North Pacific Research Board FX We thank James Ianelli, Mathieu Woillez, and two anonymous reviewers for comments on earlier drafts of this manuscript. This research was supported by a grant from the North Pacific Research Board. NR 27 TC 3 Z9 3 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD AUG PY 2012 VL 125 BP 289 EP 299 DI 10.1016/j.fishres.2012.03.003 PG 11 WC Fisheries SC Fisheries GA 953EG UT WOS:000304849100031 ER PT J AU Aveline, DC Baumgartel, L Ahn, B Yu, N AF Aveline, David C. Baumgartel, Lukas Ahn, Byungmin Yu, Nan TI Focused ion beam engineered whispering gallery mode resonators with open cavity structure SO OPTICS EXPRESS LA English DT Article ID MICRODISK RESONATORS; RAYLEIGH-SCATTERING; WAVE-GUIDES; FABRICATION; MICROCAVITIES; MICROSPHERES; CHIP AB We report the realization of an open cavity whispering gallery mode optical resonator, in which the circulating light traverses a free space gap. We utilize focused ion beam microfabrication to precisely cut a 10 m m wide notch into the perimeter of a crystalline disc. We have shown that this modified resonator structure supports high quality modes, and demonstrated qualify factor, Q similar or equal to 10(6), limited by the notch surface roughness due to the ion milling process. Furthermore, we investigated the spatial profile of the modes inside the open cavity with a microfabricated probe mechanism. This new type of resonator structure facilitates interaction of the cavity's optical field with mechanical resonators as well as individual atoms or molecules. (C) 2012 Optical Society of America C1 [Aveline, David C.; Baumgartel, Lukas; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Baumgartel, Lukas; Ahn, Byungmin] Univ So Calif, Los Angeles, CA 90089 USA. RP Aveline, DC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM daveline@jpl.nasa.gov RI Ahn, Byungmin/B-3845-2010 OI Ahn, Byungmin/0000-0002-0866-6398 FU National Aeronautics and Space Administration; NASA's Center Innovation Fund; JPL's Research and Technology Development Program FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration, with support from NASA's Center Innovation Fund and JPL's Research and Technology Development Program. FIB and SEM were performed at USC's Center for Electron Microscopy and Microanalysis (CEMMA). The authors thank Thanh Le, I. S. Grudinin, D. Strekalov, R. J.Thompson, and B. C. Regan for helpful discussions and contributions. NR 24 TC 9 Z9 9 U1 2 U2 24 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 JUL 30 PY 2012 VL 20 IS 16 BP 18091 EP 18096 DI 10.1364/OE.20.018091 PG 6 WC Optics SC Optics GA 986PR UT WOS:000307356300077 PM 23038357 ER PT J AU Katz, A Sankaran, V AF Katz, Aaron Sankaran, Venkateswaran TI High aspect ratio grid effects on the accuracy of Navier-Stokes solutions on unstructured meshes SO COMPUTERS & FLUIDS LA English DT Article; Proceedings Paper CT 6th International Conference on Computational Fluid Dynamics (ICCFD) CY JUL 12-16, 2010 CL St Petersburg, RUSSIA SP Aerosp Res & Dev, European Off, Natl Aeronaut & Space Adm DE Computational fluid dynamics; Mesh quality; Method of manufactured solutions; Unstructured grids; High aspect-ratio grids ID VERIFICATION; CODE AB The method of manufactured solutions is used to evaluate the stability and accuracy of several unstructured discretization schemes in the presence of high-aspect ratio grids. Both inviscid and viscous discretizations are studied by systematically varying parameters such as the aspect ratio, mesh stretching, curvature, skewness, and non-planar faces. For the inviscid terms, gradient reconstruction based on cell least squares and nodal Green-Gauss are considered. In particular, high curvature grids are shown to lead to instabilities with both classes of schemes and a new Green-Gauss scheme based on nodal projection is developed that retains stability and formal second-order accuracy under all conditions. A further advantage of the nodal Green-Gauss schemes is that the nodal values can be used in the viscous discretization as well. All the viscous schemes tested here are demonstrated to preserve second-order accuracy. Finally, for three-dimensional meshes, triangulation of non-planar faces is found to be necessary to preserve second-order accuracy. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Katz, Aaron; Sankaran, Venkateswaran] USA, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA 94035 USA. RP Katz, A (reprint author), NASA, Ames Res Ctr, M-S 215-1, Moffett Field, CA 94035 USA. EM akatz@merlin.arc.nasa.gov RI Katz, Aaron/I-8244-2015 OI Katz, Aaron/0000-0003-2739-9384 NR 23 TC 5 Z9 6 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 J9 COMPUT FLUIDS JI Comput. Fluids PD JUL 30 PY 2012 VL 65 SI SI BP 66 EP 79 DI 10.1016/j.compfluid.2012.02.012 PG 14 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 994IM UT WOS:000307924100008 ER PT J AU Karasik, BS Pereverzev, SV Soibel, A Santavicca, DF Prober, DE Olaya, D Gershenson, ME AF Karasik, Boris S. Pereverzev, Sergey V. Soibel, Alexander Santavicca, Daniel F. Prober, Daniel E. Olaya, David Gershenson, Michael E. TI Energy-resolved detection of single infrared photons with lambda=8 mu m using a superconducting microbolometer SO APPLIED PHYSICS LETTERS LA English DT Article ID TRANSITION-EDGE SENSORS; ELECTROTHERMAL FEEDBACK; ASTROPHYSICS; EFFICIENCY; COUNTER AB We report on the detection of single photons with gamma = 8 mu m using a superconducting hot-electron microbolometer. The sensing element is a titanium transition-edge sensor with a volume similar to 0.1 mu m(3) fabricated on a silicon substrate. Poisson photon counting statistics including simultaneous detection of 3 photons was observed. The width of the photon-number peaks was 0.11 eV, 70% of the photon energy, at 50-100 mK. This achieved energy resolution is one of the best figures reported so far for superconducting devices. Such devices can be suitable for single-photon calorimetric spectroscopy throughout the mid-infrared and even the far-infrared. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4739839] C1 [Karasik, Boris S.; Pereverzev, Sergey V.; Soibel, Alexander] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Santavicca, Daniel F.; Prober, Daniel E.] Yale Univ, New Haven, CT 06520 USA. [Olaya, David; Gershenson, Michael E.] Rutgers State Univ, Piscataway, NJ 08854 USA. RP Karasik, BS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM boris.s.karasik@jpl.nasa.gov RI Soibel, Alexander/A-1313-2007; Karasik, Boris/C-5918-2011 FU Yale University; National Aeronautics and Space Administration (NASA) [NNG04GD55G]; Rutgers Academic Excellence Fund; NSF [ECS-0608842]; [NSF-DMR-0907082]; [NSF-CHE-0616875] FX We thank A. G. Kozorezov and A. V. Sergeev for discussion and comments and J. Kawamura for providing the superconducting solenoid. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautical and Space Administration. The work at Yale University was supported in part by NSF-DMR-0907082, NSF-CHE-0616875, and Yale University. The research at Rutgers University was supported in part by the National Aeronautics and Space Administration (NASA) grant NNG04GD55G, the Rutgers Academic Excellence Fund, and the NSF grant ECS-0608842. NR 30 TC 12 Z9 12 U1 1 U2 17 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUL 30 PY 2012 VL 101 IS 5 AR 052601 DI 10.1063/1.4739839 PG 5 WC Physics, Applied SC Physics GA 991BU UT WOS:000307676600049 ER PT J AU Simms, AR Ivins, ER DeWitt, R Kouremenos, P Simkins, LM AF Simms, Alexander R. Ivins, Erik R. DeWitt, Regina Kouremenos, Peter Simkins, Lauren M. TI Timing of the most recent Neoglacial advance and retreat in the South Shetland Islands, Antarctic Peninsula: insights from raised beaches and Holocene uplift rates SO QUATERNARY SCIENCE REVIEWS LA English DT Review DE Glacial rebound; Antarctica; Little Ice Age; Sea level; Climate; Optically stimulated luminescence ID KING-GEORGE-ISLAND; RELATIVE SEA-LEVEL; OPTICALLY STIMULATED LUMINESCENCE; WEST ANTARCTICA; ICE-SHELF; PALEONTOLOGICAL EVIDENCE; GLACIAL HISTORY; GLACIOMARINE SEDIMENTATION; LIVINGSTON-ISLAND; MAXWELL BAY AB The timing of the most recent Neoglacial advance in the Antarctic Peninsula is important for establishing global climate teleconnections and providing important post-glacial rebound corrections to gravity-based satellite measurements of ice loss. However, obtaining accurate ages from terrestrial geomorphic and sedimentary indicators of the most recent Neoglacial advance in Antarctica has been hampered by the lack of historical records and the difficulty of dating materials in Antarctica. Here we use a new approach to dating flights of raised beaches in the South Shetland Islands of the northern Antarctic Peninsula to bracket the age of a Neoglacial advance that occurred between 1500 and 1700 AD, broadly synchronous with compilations for the timing of the Little Ice Age in the northern hemisphere. Our approach is based on optically stimulated luminescence of the underside of buried cobbles to obtain the age of beaches previously shown to have been deposited immediately inside and outside the moraines of the most recent Neoglacial advance. In addition, these beaches mark the timing of an apparent change in the rate of isostatic rebound thought to be in response to the same glacial advance within the South Shetland Islands. We use a Maxwell viscoelastic model of glacial-isostatic adjustment (GIA) to determine whether the rates of uplift calculated from the raised beaches are realistic given the limited constraints on the ice advance during this most recent Neoglacial advance. Our rebound model suggests that the subsequent melting of an additional 16-22% increase in the volume of ice within the South Shetland Islands would result in a subsequent uplift rate of 12.5 mm/yr that lasted until 1840 AD resulting in a cumulative uplift of 2.5 m. This uplift rate and magnitude are in close agreement with observed rates and magnitudes calculated from the raised beaches since the most recent Neoglacial advance along the South Shetland Islands and falls within the range of uplift rates from similar settings such as Alaska. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Simms, Alexander R.; Simkins, Lauren M.] Univ Calif Santa Barbara, Dept Earth Sci, Santa Barbara, CA 93106 USA. [Ivins, Erik R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [DeWitt, Regina] Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. [Kouremenos, Peter] BP Canada, Edmonton, AB T5C 0N5, Canada. RP Simms, AR (reprint author), Univ Calif Santa Barbara, Dept Earth Sci, 1006 Webb Hall, Santa Barbara, CA 93106 USA. EM asimms@geol.ucsb.edu; Erik.R.Ivins@jpl.nasa.gov; dewittr@ecu.edu; pkouremenos@yahoo.ca; lauren_e_miller@umail.ucsb.edu OI DeWitt, Regina/0000-0003-2876-5489 FU National Science Foundation [OPP-0724929, 0838781]; NASA FX The authors would like to thank Annie Drewry and the rest of the science party and crew of the R/V Nathaniel B. Palmer NBP0703 cruise for their help in collecting the samples. The authors also thank Dr. Eric Benton for the gamma spectrometry measurements. We benefited from discussion of active rift-shoulder tectonics with Gilles Peltzer. This project was funded by the National Science Foundation grants #OPP-0724929 and 0838781 to ARS and RD. Some of this research was supported by NASA's Earth Surface and Interior Focus Area, NASA's Cryosphere Program and was performed at the Jet Propulsion Laboratory, California Institute of Technology. NR 101 TC 16 Z9 16 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD JUL 30 PY 2012 VL 47 BP 41 EP 55 DI 10.1016/j.quascirev.2012.05.013 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 978GR UT WOS:000306729300004 ER PT J AU Palumbo, D AF Palumbo, Dan TI Determining correlation and coherence lengths in turbulent boundary layer flight data SO JOURNAL OF SOUND AND VIBRATION LA English DT Article ID WALL-PRESSURE-FLUCTUATIONS; SPECTRUM; BENEATH; FIELD; MODEL; AIRCRAFT; FEATURES; NUMBERS AB Wall pressure data acquired during flight tests at several flight conditions are analysed and the correlation and coherence lengths of the data reported. It is found that the correlation and coherence lengths are influenced by the origin of the structure producing the pressure and the frequency bandwidth over which the analyses are performed. It is shown how the frequency bandwidth biases the correlation length and how the convection of the pressure field might reduce the coherence measured between sensors. A convected form of the cross correlation and cross spectrum is introduced to compensate for the effects of convection. Coherence lengths measured in the streamwise direction appear much longer than expected. Coherent structures detected using the convected cross correlation do not exhibit an exponential coherent power decay. Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Palumbo, D (reprint author), NASA, Langley Res Ctr, MS 463, Hampton, VA 23681 USA. EM d.l.palumbo@nasa.gov NR 25 TC 13 Z9 13 U1 0 U2 5 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X J9 J SOUND VIB JI J. Sound Vibr. PD JUL 30 PY 2012 VL 331 IS 16 BP 3721 EP 3737 DI 10.1016/j.jsv.2012.03.015 PG 17 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 952JY UT WOS:000304790000004 ER PT J AU Thomson, BJ Bussey, DBJ Neish, CD Cahill, JTS Heggy, E Kirk, RL Patterson, GW Raney, RK Spudis, PD Thompson, TW Ustinov, EA AF Thomson, B. J. Bussey, D. B. J. Neish, C. D. Cahill, J. T. S. Heggy, E. Kirk, R. L. Patterson, G. W. Raney, R. K. Spudis, P. D. Thompson, T. W. Ustinov, E. A. TI An upper limit for ice in Shackleton crater as revealed by LRO Mini-RF orbital radar SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LUNAR SOUTH-POLE; WATER ICE; MOON; CHANDRAYAAN-1 AB Although diverse measurements have indicated H+, OH-, or H2O species in the lunar polar regions, pinpointing its location, form, and abundance in specific reservoirs has proven elusive. Here we report on the first orbital radar measurements of Shackleton crater near the lunar south pole. Mini-RF observations indicate a patchy, heterogeneous enhancement in CPR (circular polarization ratio) on the crater walls whose strength decreases with depth toward the crater floor, a result that is most consistent with a roughness effect due to less mature regolith present on the crater wall slopes. However, the results do not rule out a modest ice contribution, and an upper limit of similar to 5-10 wt% H2O ice (up to 30 vol.%) present in the uppermost meter of regolith is also consistent with the observations. C1 [Thomson, B. J.] Boston Univ, Ctr Remote Sensing, Boston, MA 02155 USA. [Bussey, D. B. J.; Neish, C. D.; Cahill, J. T. S.; Patterson, G. W.; Raney, R. K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Heggy, E.; Thompson, T. W.; Ustinov, E. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kirk, R. L.] US Geol Survey, Flagstaff, AZ 86001 USA. [Spudis, P. D.] Lunar & Planetary Inst, Houston, TX 77058 USA. RP Thomson, BJ (reprint author), Boston Univ, Ctr Remote Sensing, 725 Commonwealth Ave,Room 433, Boston, MA 02155 USA. EM bjt@bu.edu RI Neish, Catherine/G-6321-2012; Cahill, Joshua/I-3656-2012; Heggy, Essam/E-8250-2013; Ustinov, Eugene/D-1350-2015; Patterson, Gerald/E-7699-2015; OI Cahill, Joshua/0000-0001-6874-5533; Heggy, Essam/0000-0001-7476-2735; Ustinov, Eugene/0000-0003-0227-4286; Thomson, Bradley/0000-0001-8635-8932 NR 26 TC 15 Z9 17 U1 0 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 28 PY 2012 VL 39 AR L14201 DI 10.1029/2012GL052119 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 980WP UT WOS:000306925200001 ER PT J AU Jiang, X Chahine, MT Li, QB Liang, MC Olsen, ET Chen, LL Wang, JQ Yung, YL AF Jiang, Xun Chahine, Moustafa T. Li, Qinbin Liang, Maochang Olsen, Edward T. Chen, Luke L. Wang, Jingqian Yung, Yuk L. TI CO2 semiannual oscillation in the middle troposphere and at the surface SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID ATMOSPHERIC CARBON-DIOXIDE; MODEL; CYCLE; SINKS; FLUX AB Using in situ measurements, we find a semiannual oscillation (SAO) in the midtropospheric and surface CO2. Chemistry transport models (2-D Caltech/JPL model, 3-D GEOS-Chem, and 3-D MOZART-2) are used to investigate possible sources for the SAO signal in the midtropospheric and surface CO2. From model sensitivity studies, it is revealed that the SAO signal in the midtropospheric CO2 originates mainly from surface CO2 with a small contribution from transport fields. It is also found that the source for the SAO signal in surface CO2 is mostly related to the CO2 exchange between the biosphere and the atmosphere. By comparing model CO2 with in situ CO2 measurements at the surface, we find that models are able to capture both annual and semiannual cycles well at the surface. Model simulations of the annual and semiannual cycles of CO2 in the tropical middle troposphere agree reasonably well with aircraft measurements. C1 [Jiang, Xun; Wang, Jingqian] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA. [Chahine, Moustafa T.; Olsen, Edward T.; Chen, Luke L.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA USA. [Li, Qinbin] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Liang, Maochang] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Jiang, X (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA. EM xjiang4@mail.uh.edu RI Chem, GEOS/C-5595-2014 FU JPL [G99694, P765982]; NSC [98-2111-M-001-014-MY3] FX We thank two anonymous reviewers and the Associate Editor for the helpful comments. X. Jiang is supported by JPL grant G99694. M. Liang is supported by NSC grant 98-2111-M-001-014-MY3 to Academia Sinica. Y. L. Yung is supported by JPL grant P765982 to the California Institute of Technology. NR 25 TC 9 Z9 9 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD JUL 28 PY 2012 VL 26 AR GB3006 DI 10.1029/2011GB004118 PG 9 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 980XM UT WOS:000306927500001 ER PT J AU Houborg, R Rodell, M Li, BL Reichle, R Zaitchik, BF AF Houborg, Rasmus Rodell, Matthew Li, Bailing Reichle, Rolf Zaitchik, Benjamin F. TI Drought indicators based on model-assimilated Gravity Recovery and Climate Experiment (GRACE) terrestrial water storage observations SO WATER RESOURCES RESEARCH LA English DT Article ID CATCHMENT-BASED APPROACH; LAND-SURFACE PROCESSES; SOIL-MOISTURE; RIVER-BASINS; SYSTEM; EVAPOTRANSPIRATION; PRECIPITATION; VARIABILITY; IMPACT AB The Gravity Recovery and Climate Experiment (GRACE) twin satellites observe time variations in Earth's gravity field which yield valuable information about changes in terrestrial water storage (TWS). GRACE is characterized by low spatial (>150,000 km(2)) and temporal (> 10 days) resolution but has the unique ability to sense water stored at all levels (including groundwater) systematically and continuously. The GRACE Data Assimilation System (DAS), based on the Catchment Land Surface Model (CLSM), enhances the value of the GRACE water storage data by enabling spatial and temporal downscaling and vertical decomposition into moisture components (i.e., groundwater, soil moisture, and snow), which individually are more useful for scientific applications. In this study, GRACE DAS was applied to North America, and GRACE-based drought indicators were developed as part of a larger effort to investigate the possibility of more comprehensive and objective identification of drought conditions by integrating spatially, temporally, and vertically disaggregated GRACE data into the U. S. and North American Drought Monitors. Previously, the drought monitors lacked objective information on deep soil moisture and groundwater conditions, which are useful indicators of drought. Extensive data sets of groundwater storage from U. S. Geological Survey monitoring wells and soil moisture from the Soil Climate Analysis Network were used to assess improvements in the hydrological modeling skill resulting from the assimilation of GRACE TWS data. The results point toward modest, but statistically significant, improvements in the hydrological modeling skill across major parts of the United States, highlighting the potential value of a GRACE-assimilated water storage field for improving drought detection. C1 [Houborg, Rasmus] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, Climate Risk Management Unit, I-21027 Ispra, Italy. [Houborg, Rasmus; Li, Bailing] E Syst Sci Interdisciplinary Ctr, College Pk, MD USA. [Rodell, Matthew; Li, Bailing; Reichle, Rolf] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zaitchik, Benjamin F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. RP Houborg, R (reprint author), Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, Climate Risk Management Unit, Via Enrico Fermi 2749, I-21027 Ispra, Italy. EM rasmus.houborg@jrc.ec.europa.eu RI Reichle, Rolf/E-1419-2012; Zaitchik, Benjamin/B-9461-2013; Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 FU NASA FX This project was supported by NASA's Applied Sciences program. VIC data were processed and kindly made available by Huilin Gao. GRACE land data were processed by Sean Swenson, supported by the NASA MEASURES Program, and are available at http://grace.jpl.nasa.gov. NR 58 TC 73 Z9 76 U1 2 U2 65 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 JUL 28 PY 2012 VL 48 AR W07525 DI 10.1029/2011WR011291 PG 17 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 980PT UT WOS:000306906100001 ER PT J AU Weng, ESS Luo, YQ Wang, WL Wang, H Hayes, DJ McGuire, AD Hastings, A Schimel, DS AF Weng, Ensheng S. Luo, Y. Q. Wang, Weile Wang, Han Hayes, Daniel J. McGuire, A. David Hastings, Alan Schimel, David S. TI Ecosystem carbon storage capacity as affected by disturbance regimes: A general theoretical model SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID NET PRIMARY PRODUCTIVITY; OLD-GROWTH FORESTS; CLIMATE-CHANGE; CONTINENTAL-SCALE; NITROGEN STORAGE; PONDEROSA PINE; GLOBAL-MODEL; FIRE; BALANCE; LANDSCAPE AB Disturbances have been recognized as a key factor shaping terrestrial ecosystem states and dynamics. A general model that quantitatively describes the relationship between carbon storage and disturbance regime is critical for better understanding large scale terrestrial ecosystem carbon dynamics. We developed a model (REGIME) to quantify ecosystem carbon storage capacities (E[x]) under varying disturbance regimes with an analytical solution E[x] =U . tau(E) . lambda/lambda+s tau(1), where U is ecosystem carbon influx, tau(E) is ecosystem carbon residence time, and tau(1) is the residence time of the carbon pool affected by disturbances (biomass pool in this study). The disturbance regime is characterized by the mean disturbance interval (lambda) and the mean disturbance severity (s). It is a Michaelis-Menten-type equation illustrating the saturation of carbon content with mean disturbance interval. This model analytically integrates the deterministic ecosystem carbon processes with stochastic disturbance events to reveal a general pattern of terrestrial carbon dynamics at large scales. The model allows us to get a sense of the sensitivity of ecosystems to future environmental changes just by a few calculations. According to the REGIME model, for example, approximately 1.8 Pg C will be lost in the high-latitude regions of North America (>45 degrees N) if fire disturbance intensity increases around 5.7 time the current intensity to the end of the twenty-first century, which will require around 12% increases in net primary productivity (NPP) to maintain stable carbon stocks. If the residence time decreased 10% at the same time additional 12.5% increases in NPP are required to keep current C stocks. The REGIME model also lays the foundation for analytically modeling the interactions between deterministic biogeochemical processes and stochastic disturbance events. C1 [Weng, Ensheng S.; Luo, Y. Q.] Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA. [Wang, Weile] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wang, Han] Univ Oklahoma, Sch Elect & Comp Engn, Norman, OK 73019 USA. [Hayes, Daniel J.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [McGuire, A. David] Univ Alaska, US Geol Survey, Alaska Cooperat Fish & Wildlife Res Unit, Fairbanks, AK 99701 USA. [Hastings, Alan] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Schimel, David S.] NEON Inc, Boulder, CO USA. RP Weng, ESS (reprint author), Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA. EM wengensheng@gmail.com RI Weng, Ensheng/E-4390-2012; Hayes, Daniel/B-8968-2012 OI Weng, Ensheng/0000-0002-1858-4847; FU Office of Science, Department of Energy [DE-FG02-006ER64319]; Midwestern Regional Center of the National Institute for Climatic Change Research at Michigan Technological University [DE-FC02-06ER64158]; National Science Foundation [DBI 0850290, DEB 0840964, DEB 0743778, EPS 0919466] FX This research was financially supported by the Office of Science, Department of Energy (grant DE-FG02-006ER64319); by the Midwestern Regional Center of the National Institute for Climatic Change Research at Michigan Technological University under award DE-FC02-06ER64158; and by the National Science Foundation under DBI 0850290, DEB 0840964, DEB 0743778, and EPS 0919466. We thank Nikola P. Petrov of the University of Oklahoma, Jeremy W. Lichstein of the University of Florida, and Anping Chen of Princeton University for their helpful comments. NR 75 TC 12 Z9 12 U1 1 U2 44 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 JUL 27 PY 2012 VL 117 AR G03014 DI 10.1029/2012JG002040 PG 15 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 980RB UT WOS:000306909600001 ER PT J AU Iess, L Jacobson, RA Ducci, M Stevenson, DJ Lunine, JI Armstrong, JW Asmar, SW Racioppa, P Rappaport, NJ Tortora, P AF Iess, Luciano Jacobson, Robert A. Ducci, Marco Stevenson, David J. Lunine, Jonathan I. Armstrong, John W. Asmar, Sami W. Racioppa, Paolo Rappaport, Nicole J. Tortora, Paolo TI The Tides of Titan SO SCIENCE LA English DT Article ID OCEAN; ICE AB We have detected in Cassini spacecraft data the signature of the periodic tidal stresses within Titan, driven by the eccentricity (e = 0.028) of its 16-day orbit around Saturn. Precise measurements of the acceleration of Cassini during six close flybys between 2006 and 2011 have revealed that Titan responds to the variable tidal field exerted by Saturn with periodic changes of its quadrupole gravity, at about 4% of the static value. Two independent determinations of the corresponding degree-2 Love number yield k(2) = 0.589 +/- 0.150 and k(2) = 0.637 +/- 0.224 (2 sigma). Such a large response to the tidal field requires that Titan's interior be deformable over time scales of the orbital period, in a way that is consistent with a global ocean at depth. C1 [Iess, Luciano; Ducci, Marco; Racioppa, Paolo] Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerosp, I-00184 Rome, Italy. [Jacobson, Robert A.; Armstrong, John W.; Asmar, Sami W.; Rappaport, Nicole J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stevenson, David J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lunine, Jonathan I.] Cornell Univ, Dept Astron, Ithaca, NY 14850 USA. [Tortora, Paolo] Univ Bologna, DIEM II Fac Ingn, I-47121 Forli, Italy. RP Iess, L (reprint author), Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerosp, Via Eudossiana 18, I-00184 Rome, Italy. EM luciano.iess@uniroma1.it RI Tortora, Paolo/J-6191-2012; IESS, Luciano/F-4902-2011 OI Tortora, Paolo/0000-0001-9259-7673; IESS, Luciano/0000-0002-6230-5825 FU Italian Space Agency; NASA FX L.I., M.D., P.R., and P.T. acknowledge support from the Italian Space Agency. The work of R.A.J., J.W.A., S.W.A., and N.J.R. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The Doppler data used in this analysis are archived in NASA's Planetary Data System. NR 12 TC 50 Z9 51 U1 1 U2 37 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 JUL 27 PY 2012 VL 337 IS 6093 BP 457 EP 459 DI 10.1126/science.1219631 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 979FS UT WOS:000306802300040 PM 22745254 ER PT J AU Painter, TH Skiles, SM Deems, JS Bryant, AC Landry, CC AF Painter, Thomas H. Skiles, S. McKenzie Deems, Jeffrey S. Bryant, Ann C. Landry, Christopher C. TI Dust radiative forcing in snow of the Upper Colorado River Basin: 1. A 6 year record of energy balance, radiation, and dust concentrations SO WATER RESOURCES RESEARCH LA English DT Article ID CLIMATE-CHANGE; WATER; ALBEDO AB Dust in snow accelerates snowmelt through its direct reduction of snow albedo and its further indirect reduction of albedo by accelerating the growth of snow grains. Since the westward expansion of the United States that began in the mid-19th century, the mountain snow cover of the Colorado River Basin has been subject to five-fold greater dust loading, largely from the Colorado Plateau and Great Basin. Radiative forcing of snowmelt by dust is not captured by conventional micrometeorological measurements, and must be monitored by a more comprehensive suite of radiation instruments. Here we present a 6 year record of energy balance and detailed radiation measurements in the Senator Beck Basin Study Area, San Juan Mountains, Colorado, USA. Data include broadband irradiance, filtered irradiance, broadband reflected flux, filtered reflected flux, broadband and visible albedo, longwave irradiance, wind speed, relative humidity, and air temperatures. The gradient of the snow surface is monitored weekly and used to correct albedo measurements for geometric effects. The snow is sampled weekly for dust concentrations in plots immediately adjacent to each tower over the melt season. Broadband albedo in the last weeks of snow cover ranged from 0.33 to 0.55 across the 6 years and two sites. Total end of year dust concentration in the top 3 cm of the snow column ranged from 0.23 mg g(-1) to 4.16 mg g(-1). These measurements enable monitoring and modeling of dust and climate-driven snowmelt forcings in the Upper Colorado River Basin. C1 [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Painter, Thomas H.; Skiles, S. McKenzie] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA. [Painter, Thomas H.; Skiles, S. McKenzie] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Deems, Jeffrey S.] Natl Snow & Ice Data Ctr, Boulder, CO USA. [Deems, Jeffrey S.] NOAA Western Water Assessment, Boulder, CO USA. [Bryant, Ann C.] Univ Utah, Dept Geog, Salt Lake City, UT USA. [Landry, Christopher C.] Ctr Snow & Avalanche Studies, Silverton, CO USA. RP Painter, TH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM thomas.painter@jpl.nasa.gov RI Painter, Thomas/B-7806-2016; Deems, Jeffrey/E-6484-2016 OI Deems, Jeffrey/0000-0002-3265-8670 FU National Science Foundation [ATM04323237, ATM0431955]; NASA [NNX10AO97G] FX This work was funded by the National Science Foundation grants ATM04323237 and ATM0431955, and NASA project NNX10AO97G. We acknowledge the assistance of Andrew Barrett in data processing. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We thank Jeff Dozier, Steve Warren, and an anonymous reviewer for their suggestions that improved this manuscript. NR 19 TC 47 Z9 48 U1 2 U2 35 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 JUL 26 PY 2012 VL 48 AR W07521 DI 10.1029/2012WR011985 PG 14 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 980PQ UT WOS:000306905800001 ER PT J AU Skiles, SM Painter, TH Deems, JS Bryant, AC Landry, CC AF Skiles, S. McKenzie Painter, Thomas H. Deems, Jeffrey S. Bryant, Ann C. Landry, Christopher C. TI Dust radiative forcing in snow of the Upper Colorado River Basin: 2. Interannual variability in radiative forcing and snowmelt rates SO WATER RESOURCES RESEARCH LA English DT Article ID HYPERSPECTRAL ANALYSIS; ENERGY EXCHANGE; ALPINE REGION; SIERRA-NEVADA; GRAIN-SIZE; CLIMATE; SURFACE; CONTAMINATION; REFLECTANCE; DEPOSITION AB Here we present the radiative and snowmelt impacts of dust deposition to snow cover using a 6-year energy balance record (2005-2010) at alpine and subalpine micrometeorological towers in the Senator Beck Basin Study Area (SBBSA) in southwestern Colorado, USA. These results follow from the measurements described in part I. We simulate the evolution of snow water equivalent at each station under scenarios of observed and dust-free conditions, and +2 degrees C and +4 degrees C melt-season temperature perturbations to these scenarios. Over the 6 years of record, daily mean dust radiative forcing ranged from 0 to 214 W m(-2), with hourly peaks up to 409 W m(-2). Mean springtime dust radiative forcings across the period ranged from 31 to 49 W m(-2) at the alpine site and 45 to 75 W m(-2) at the subalpine site, in turn shortening snow cover duration by 21 to 51 days. The dust-advanced loss of snow cover (days) is linearly related to total dust concentration at the end of snow cover, despite temporal variability in dust exposure and solar irradiance. Under clean snow conditions, the temperature increases shorten snow cover by 5-18 days, whereas in the presence of dust they only shorten snow duration by 0-6 days. Dust radiative forcing also causes faster and earlier peak snowmelt outflow with daily mean snowpack outflow doubling under the heaviest dust conditions. On average, snow cover at the towers is lost 2.5 days after peak outflow in dusty conditions, and 1-2 weeks after peak outflow in clean conditions. C1 [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Skiles, S. McKenzie; Painter, Thomas H.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA. [Skiles, S. McKenzie; Painter, Thomas H.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90024 USA. [Deems, Jeffrey S.] Natl Snow & Ice Data Ctr, Boulder, CO USA. [Deems, Jeffrey S.] NOAA Western Water Assessment, Boulder, CO USA. [Bryant, Ann C.] Univ Utah, Dept Geog, Salt Lake City, UT USA. [Landry, Christopher C.] Ctr Snow & Avalanche Studies, Silverton, CO USA. RP Painter, TH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM thomas.painter@jpl.nasa.gov RI Painter, Thomas/B-7806-2016; Deems, Jeffrey/E-6484-2016 OI Deems, Jeffrey/0000-0002-3265-8670 FU National Science Foundation [ATM04323237, ATM0431955]; NASA [NNX10AO97G] FX This work was funded by the National Science Foundation grants ATM04323237 and ATM0431955, and NASA project NNX10AO97G. We acknowledge the assistance of Andrew Barrett in data processing. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We thank Jeff Dozier, Steve Warren, and an anonymous reviewer for their suggestions that improved this manuscript. NR 23 TC 50 Z9 50 U1 2 U2 50 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 JUL 26 PY 2012 VL 48 AR W07522 DI 10.1029/2012WR011986 PG 11 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 980PQ UT WOS:000306905800002 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Ackermann, M Adams, J Aguilar, JA Ahlers, M Altmann, D Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Baum, V Bay, R Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Bell, M Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Brayeur, L Brown, AM Buitink, S Caballero-Mora, KS Carson, M Casier, M Chirkin, D Christy, B Clevermann, F Cohen, S Cowen, DF Silva, AHC D'Agostino, MV Danninger, M Daughhetee, J Davis, JC De Clercq, C Degner, T Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dreyer, J Dumm, JP Dunkman, M Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Flis, S Franckowiak, A Franke, R Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Gora, D Grant, D Gross, A Grullon, S Gurtner, M Ha, C Ismail, AH Hallgren, A Halzen, F Hanson, K Heereman, D Heimann, P Heinen, D Helbing, K Hellauer, R Hickford, S Hill, GC Hoffman, KD Hoffmann, B Homeier, A Hoshina, K Huelsnitz, W Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Japaridze, GS Johansson, H Kappes, A Karg, T Karle, A Kiryluk, J Kislat, F Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, S Koskinen, DJ Kowalski, M Krasberg, M Kroll, G Kunnen, J Kurahashi, N Kuwabara, T Labare, M Laihem, K Landsman, H Larson, MJ Lauer, R Lunemann, J Madsen, J Maruyama, R Mase, K Matis, HS Meagher, K Merck, M Meszaros, P Meures, T Miarecki, S Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Nowicki, SC Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Panknin, S Paul, L de los Heros, CP Pieloth, D Posselt, J Price, PB Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Richman, M Riedel, B Rodrigues, JP Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Scheel, M Schmidt, T Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Smith, MWE Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Stuer, M Sullivan, GW Taavola, H Taboada, I Tamburro, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S van Eijndhoven, N Van Overloop, A van Santen, J Vehring, M Voge, M Walck, C Waldenmaier, T Wallraff, M Walter, M Wasserman, R Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wischnewski, R Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, C Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Zoll, M AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Altmann, D. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Baum, V. Bay, R. Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K. -H. Bell, M. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brayeur, L. Brown, A. M. Buitink, S. Caballero-Mora, K. S. Carson, M. Casier, M. Chirkin, D. Christy, B. Clevermann, F. Cohen, S. Cowen, D. F. Silva, A. H. Cruz D'Agostino, M. V. Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Degner, T. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dreyer, J. Dumm, J. P. Dunkman, M. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Gora, D. Grant, D. Gross, A. Grullon, S. Gurtner, M. Ha, C. Ismail, A. Haj Hallgren, A. Halzen, F. Hanson, K. Heereman, D. Heimann, P. Heinen, D. Helbing, K. Hellauer, R. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, B. Homeier, A. Hoshina, K. Huelsnitz, W. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobi, E. Jacobsen, J. Japaridze, G. S. Johansson, H. Kappes, A. Karg, T. Karle, A. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, S. Koskinen, D. J. Kowalski, M. Krasberg, M. Kroll, G. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Luenemann, J. Madsen, J. Maruyama, R. Mase, K. Matis, H. S. Meagher, K. Merck, M. Meszaros, P. Meures, T. Miarecki, S. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Nowicki, S. C. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Panknin, S. Paul, L. de los Heros, C. Perez Pieloth, D. Posselt, J. Price, P. B. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Richman, M. Riedel, B. Rodrigues, J. P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Scheel, M. Schmidt, T. Schoeneberg, S. Schoenwald, A. Schukraft, A. Schulte, L. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Smith, M. W. E. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Stroem, R. Stueer, M. Sullivan, G. W. Taavola, H. Taboada, I. Tamburro, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. van Eijndhoven, N. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Wasserman, R. Weaver, Ch Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, C. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Zoll, M. CA IceCube Collaboration TI Search for ultrahigh-energy tau neutrinos with IceCube SO PHYSICAL REVIEW D LA English DT Article ID INDUCED CASCADES; AMANDA; EARTH; PROPAGATION; TELESCOPES; SELECTION AB The first dedicated search for ultrahigh-energy (UHE) tau neutrinos of astrophysical origin was performed using the IceCube detector in its 22-string configuration with an instrumented volume of roughly 0: 25 km(3). The search also had sensitivity to UHE electron and muon neutrinos. After application of all selection criteria to approximately 200 live-days of data, we expect a background of 0.60 +/- 0.19(stat)(-0.58)(+0.56)(syst) events and observe three events, which after inspection, emerge as being compatible with background but are kept in the final sample. Therefore, we set an upper limit on neutrinos of all flavors from UHE astrophysical sources at 90% C.L. of E-v(2)Phi(90)(v(x)) < 16.3 x 10(-8) GeV cm(-2) sr(-1) s(-1) over an estimated primary neutrino energy range of 340 TeV to 200 PeV. C1 [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Altmann, D.; Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Heimann, P.; Heinen, D.; Hoffmann, B.; Laihem, K.; Paul, L.; Scheel, M.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Boeser, S.; Degner, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Schulte, L.; Stueer, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados. [Bechet, S.; Bertrand, D.; Hanson, K.; Heereman, D.; Meures, T.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium. [Bose, D.; Brayeur, L.; Buitink, S.; Casier, M.; De Clercq, C.; Kunnen, J.; Labare, M.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Adams, J.; Brown, A. M.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Grant, D.; Nowicki, S. C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Aguilar, J. A.; Montaruli, T.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Abbasi, R.; Ahlers, M.; Andeen, K.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; Merck, M.; Morse, R.; O'Murchadha, A.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Baum, V.; Koepke, L.; Kroll, G.; Luenemann, J.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany. [Bai, X.; Berghaus, P.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Bai, X.; Berghaus, P.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Kiryluk, J.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bell, M.; Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Koskinen, D. J.; Larson, M. J.; Meszaros, P.; Rutledge, D.; Smith, M. W. E.; Wasserman, R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Botner, O.; Engdegard, O.; Hallgren, A.; de los Heros, C. Perez; Stroem, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Ackermann, M.; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Silva, A. H. Cruz; Franke, R.; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kislat, F.; Lauer, R.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Walter, M.; Wischnewski, R.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Montaruli, T.] Dipartimento Fis, Sez INFN, I-70126 Bari, Italy. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Seo, SH (reprint author), Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. EM seo@fysik.su.se RI Hallgren, Allan/A-8963-2013; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Wiebusch, Christopher/G-6490-2012; Tjus, Julia/G-8145-2012; Kowalski, Marek/G-5546-2012; Tamburro, Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Taavola, Henric/B-4497-2011; OI Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Wiebusch, Christopher/0000-0002-6418-3008; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Perez de los Heros, Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886 FU U.S. National Science Foundation-Office of Polar Programs; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison; Open Science Grid (OSG) grid infrastructure; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI); Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute; Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Swiss National Science Foundation (SNSF), Switzerland; U.S. Department of Energy; National Science and Engineering Research Council of Canada; Swedish Research Council; Japan Society for Promotion of Science (JSPS) FX We acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland. NR 49 TC 16 Z9 16 U1 0 U2 6 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 JUL 26 PY 2012 VL 86 IS 2 AR 022005 DI 10.1103/PhysRevD.86.022005 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 980YL UT WOS:000306930000001 ER PT J AU Sanchis-Ojeda, R Fabrycky, DC Winn, JN Barclay, T Clarke, BD Ford, EB Fortney, JJ Geary, JC Holman, MJ Howard, AW Jenkins, JM Koch, D Lissauer, JJ Marcy, GW Mullally, F Ragozzine, D Seader, SE Still, M Thompson, SE AF Sanchis-Ojeda, Roberto Fabrycky, Daniel C. Winn, Joshua N. Barclay, Thomas Clarke, Bruce D. Ford, Eric B. Fortney, Jonathan J. Geary, John C. Holman, Matthew J. Howard, Andrew W. Jenkins, Jon M. Koch, David Lissauer, Jack J. Marcy, Geoffrey W. Mullally, Fergal Ragozzine, Darin Seader, Shawn E. Still, Martin Thompson, Susan E. TI Alignment of the stellar spin with the orbits of a three-planet system SO NATURE LA English DT Article ID EXTRASOLAR PLANETS; STAR; STARSPOTS; TRANSITS; MASS AB The Sun's equator and the planets' orbital planes are nearly aligned, which is presumably a consequence of their formation from a single spinning gaseous disk. For exoplanetary systems this well-aligned configuration is not guaranteed: dynamical interactions may tilt planetary orbits, or stars may be misaligned with the protoplanetary disk through chaotic accretion(1), magnetic interactions(2) or torques from neighbouring stars. Indeed, isolated 'hot Jupiters' are often misaligned and even orbiting retrograde(3,4). Here we report an analysis of transits of planets over starspots(5-7) on the Sun-like star Kepler-30 (ref. 8), and show that the orbits of its three planets are aligned with the stellar equator. Furthermore, the orbits are aligned with one another to within a few degrees. This configuration is similar to that of our Solar System, and contrasts with the isolated hot Jupiters. The orderly alignment seen in the Kepler-30 system suggests that high obliquities are confined to systems that experienced disruptive dynamical interactions. Should this be corroborated by observations of other coplanar multi-planet systems, then star-disk misalignments would be ruled out as the explanation for the high obliquities of hot Jupiters, and dynamical interactions would be implicated as the origin of hot Jupiters. C1 [Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Fabrycky, Daniel C.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Barclay, Thomas; Clarke, Bruce D.; Jenkins, Jon M.; Koch, David; Lissauer, Jack J.; Mullally, Fergal; Seader, Shawn E.; Still, Martin; Thompson, Susan E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Clarke, Bruce D.; Jenkins, Jon M.; Mullally, Fergal; Seader, Shawn E.; Thompson, Susan E.] SETI Inst, Mountain View, CA USA. [Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Geary, John C.; Holman, Matthew J.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howard, Andrew W.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Sanchis-Ojeda, R (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM rsanchis86@gmail.com; daniel.fabrycky@gmail.com RI Sanchis-Ojeda, Roberto/B-6574-2013; Ragozzine, Darin/C-4926-2013; OI Sanchis-Ojeda, Roberto/0000-0002-6193-972X; Fortney, Jonathan/0000-0002-9843-4354; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASA through Hubble Fellowship [HF-51272.01-A]; STScI; NASA through the Kepler Participating Scientist programme FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission was provided by NASA's Science Mission Directorate. The data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. S. Albrecht, E. Agol, J. A. Carter, L. Doyle and A. Shporer provided comments on the manuscript. D. C. F. acknowledges NASA support through Hubble Fellowship grant HF-51272.01-A, awarded by STScI. D. R. acknowledges the Harvard Institute for Theory and Computation. E. B. F., M. J. H. and J.N.W. acknowledge NASA support through the Kepler Participating Scientist programme. NR 20 TC 92 Z9 92 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 JUL 26 PY 2012 VL 487 IS 7408 BP 449 EP 453 DI 10.1038/nature11301 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 979KD UT WOS:000306815300031 PM 22836999 ER PT J AU Kasting, JF Catling, DC Zahnle, K AF Kasting, James F. Catling, David C. Zahnle, Kevin TI Atmospheric oxygenation and volcanism SO NATURE LA English DT Letter ID BLACK SMOKERS; PRESSURE C1 [Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Catling, David C.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Catling, David C.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Zahnle, Kevin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kasting, JF (reprint author), Penn State Univ, Dept Geosci, 443 Deike, University Pk, PA 16802 USA. EM kasting@essc.psu.edu RI Catling, David/D-2082-2009; OI Catling, David/0000-0001-5646-120X NR 6 TC 6 Z9 6 U1 1 U2 38 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 26 PY 2012 VL 487 IS 7408 BP E1 EP E1 DI 10.1038/nature11274 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 979KD UT WOS:000306815300001 PM 22837006 ER PT J AU Hanasoge, SM Duvall, TL Sreenivasan, KR AF Hanasoge, Shravan M. Duvall, Thomas L., Jr. Sreenivasan, Katepalli R. TI Anomalously weak solar convection SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE imaging; thermal wind balance; Reynolds stresses; inverse problem ID TIME-DISTANCE HELIOSEISMOLOGY; DIFFERENTIAL ROTATION; SIMULATIONS; INTERIOR; KERNELS; STARS; MODEL; ZONE AB Convection in the solar interior is thought to comprise structures on a spectrum of scales. This conclusion emerges from phenomenological studies and numerical simulations, though neither covers the proper range of dynamical parameters of solar convection. Here, we analyze observations of the wavefield in the solar photosphere using techniques of time-distance helioseismology to image flows in the solar interior. We downsample and synthesize 900 billion wavefield observations to produce 3 billion cross-correlations, which we average and fit, measuring 5 million wave travel times. Using these travel times, we deduce the underlying flow systems and study their statistics to bound convective velocity magnitudes in the solar interior, as a function of depth and spherical-harmonic degree l. Within the wavenumber band l < 60, convective velocities are 20-100 times weaker than current theoretical estimates. This constraint suggests the prevalence of a different paradigm of turbulence from that predicted by existing models, prompting the question: what mechanism transports the heat flux of a solar luminosity outwards? Advection is dominated by Coriolis forces for wavenumbers l < 60, with Rossby numbers smaller than approximately 10(-2) at r/R-circle dot = 0.96, suggesting that the Sun may be a much faster rotator than previously thought, and that large-scale convection may be quasi-geostrophic. The fact that isorotation contours in the Sun are not coaligned with the axis of rotation suggests the presence of a latitudinal entropy gradient. C1 [Hanasoge, Shravan M.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Hanasoge, Shravan M.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Duvall, Thomas L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Sreenivasan, Katepalli R.] NYU, Courant Inst Math Sci, New York, NY 10012 USA. RP Hanasoge, SM (reprint author), Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. EM krs3@nyu.edu FU NASA [NNX11AB63G] FX All computing was performed on NASA Ames super-computers: Schirra and Pleiades. S. M. H. acknowledges support from NASA Grant NNX11AB63G and thanks Courant Institute, NYU for hosting him as a visitor. Many thanks to Tim Sandstrom of the NASA-Ames visualization group for having prepared Fig. 1. Thanks to M. Schussler and M. Rempel for useful conversations. T. L. D. thanks the Stanford solar group for their hospitality. Observational data that are used in our analyses here are taken by the Helioseismic and Magnetic Imager and are publicly available at http://hmi.stanford.edu/. J. Leibacher and P. S. Cally are thanked for their careful reading of the manuscript and the considered comments that helped in improving it. We thank M. Miesch for sending us the simulation spectra. NR 29 TC 42 Z9 44 U1 0 U2 6 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 JUL 24 PY 2012 VL 109 IS 30 BP 11928 EP 11932 DI 10.1073/pnas.1206570109 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 981TD UT WOS:000306992700019 PM 22665774 ER PT J AU Saide, PE Carmichael, GR Spak, SN Minnis, P Ayers, JK AF Saide, Pablo E. Carmichael, Gregory R. Spak, Scott N. Minnis, Patrick Ayers, J. Kirk TI Improving aerosol distributions below clouds by assimilating satellite-retrieved cloud droplet number SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE air quality; indirect effect; weather prediction; stratiform cloud; microphysics ID COMMUNITY MULTISCALE AIR; VOCALS-REX; MARINE STRATOCUMULUS; SOUTHEAST PACIFIC; BOUNDARY-LAYER; WRF-CHEM; MODEL; PRECIPITATION; VARIABILITY; HEALTH AB Limitations in current capabilities to constrain aerosols adversely impact atmospheric simulations. Typically, aerosol burdens within models are constrained employing satellite aerosol optical properties, which are not available under cloudy conditions. Here we set the first steps to overcome the long-standing limitation that aerosols cannot be constrained using satellite remote sensing under cloudy conditions. We introduce a unique data assimilation method that uses cloud droplet number (N-d) retrievals to improve predicted below-cloud aerosol mass and number concentrations. The assimilation, which uses an adjoint aerosol activation parameterization, improves agreement with independent N-d observations and with in situ aerosol measurements below shallow cumulus clouds. The impacts of a single assimilation on aerosol and cloud forecasts extend beyond 24 h. Unlike previous methods, this technique can directly improve predictions of near-surface fine mode aerosols responsible for human health impacts and low-cloud radiative forcing. Better constrained aerosol distributions will help improve health effects studies, atmospheric emissions estimates, and air-quality, weather, and climate predictions. C1 [Saide, Pablo E.; Carmichael, Gregory R.; Spak, Scott N.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. [Minnis, Patrick] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Ayers, J. Kirk] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. RP Saide, PE (reprint author), Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA. EM pablo-saide@uiowa.edu RI Spak, Scott/B-7331-2008; Minnis, Patrick/G-1902-2010 OI Spak, Scott/0000-0002-8545-1411; Minnis, Patrick/0000-0002-4733-6148 FU National Science Foundation (NSF) [0748012]; Fulbright-CONICYT (Comision Nacional de Investigacion Cientifica y Tecnologica de Chile) [15093810]; NASA [NNX08AL05G, NNX11AI52G]; Department of Energy (DoE) FX We would like to acknowledge insightful comments of Marc Bocquet, Elliott Campbell, and two anonymous reviewers. We also thank all VOCALS-REx participants, specially Antony Clarke, Steve Howell and Lindsey Shank for AMS and PCASP data. This work was carried out with the aid of National Science Foundation (NSF) Grant 0748012, Fulbright-CONICYT (Comision Nacional de Investigacion Cientifica y Tecnologica de Chile) scholarship number 15093810, NASA grants NNX08AL05G and NNX11AI52G, the NASA Modeling, Analysis and Prediction (MAP) Program, and the Department of Energy (DoE) Atmospheric System Research (ASR) Program. This research was supported in part through computational resources provided by The University of Iowa, Iowa City, Iowa. NR 46 TC 13 Z9 13 U1 1 U2 22 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 24 PY 2012 VL 109 IS 30 BP 11939 EP 11943 DI 10.1073/pnas.1205877109 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 981TD UT WOS:000306992700021 PM 22778436 ER PT J AU Righter, K Ghiorso, MS AF Righter, K. Ghiorso, M. S. TI Redox systematics of a magma ocean with variable pressure-temperature gradients and composition SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE differentiation; silicate melt; isentrope; oxidation; reduction ID EQUATION-OF-STATE; ANHYDROUS PERIDOTITE KLB-1; CORE FORMATION; SILICATE MELTS; OXIDATION-STATE; OXYGEN FUGACITY; SIDEROPHILE ELEMENTS; MANTLE REDOX; EARTH; METAL AB Oxygen fugacity in metal-bearing systems controls some fundamental aspects of the geochemistry of the early Earth, such as the FeO and siderophile trace element content of the mantle, volatile species that influence atmospheric composition, and conditions for organic compounds synthesis. Redox and metal-silicate equilibria in the early Earth are sensitive to oxygen fugacity (fO(2)), yet are poorly constrained in modeling and experimentation. High pressure and temperature experimentation and modeling in metal-silicate systems usually employs an approximation approach for estimating fO(2) that is based on the ratio of Fe and FeO [called "Delta IW (ratio)" hereafter]. We present a new approach that utilizes free energy and activity modeling of the equilibrium: Fe + SiO2 + O-2 = Fe2SiO4 to calculate absolute fO(2) and relative to the iron-wustite (IW) buffer at pressure and temperature [Delta IW (P, T)]. This equilibrium is considered across a wide range of pressures and temperatures, including up to the liquidus temperature of peridotite (4,000 K at 50 GPa). Application of Delta IW (ratio) to metal-silicate experiments can be three or four orders of magnitude different from Delta IW (P, T) values calculated using free energy and activity modeling. We will also use this approach to consider the variation in oxygen fugacity in a magma ocean scenario for various thermal structures for the early Earth: hot liquidus gradient, 100 degrees C below the liquidus, hot and cool adiabatic gradients, and a cool subsolidus adiabat. The results are used to assess the effect of increasing P and T, changing silicate composition during accretion, and related to current models for accretion and core formation in the Earth. The fO(2) in a deep magma ocean scenario may become lower relative to the IW buffer at hotter and deeper conditions, which could include metal entrainment scenarios. Therefore, fO(2) may evolve from high to low fO(2) during Earth (and other differentiated bodies) accretion. Any modeling of core formation and metal-silicate equilibrium should take these effects into account. C1 [Righter, K.] Natl Aeronaut & Space Adm Johnson Space Ctr, Houston, TX 77058 USA. [Ghiorso, M. S.] OFM Res, Seattle, WA 98115 USA. RP Righter, K (reprint author), Natl Aeronaut & Space Adm Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov FU National Aeronautics and Space Administration; National Science Foundation [EAR-0838182] FX Support for this research was provided by a National Aeronautics and Space Administration Research and Technology Operating Plan from the Cosmochemistry Program to K. R. and EAR-0838182 (National Science Foundation) funding to M. Ghiorso. NR 59 TC 12 Z9 12 U1 0 U2 18 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 JUL 24 PY 2012 VL 109 IS 30 BP 11955 EP 11960 DI 10.1073/pnas.1202754109 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 981TD UT WOS:000306992700024 PM 22778438 ER PT J AU Wang, ML Hada, M Saha, J Sridharan, DM Pluth, JM Cucinotta, FA AF Wang, Minli Hada, Megumi Saha, Janapriya Sridharan, Deepa M. Pluth, Janice M. Cucinotta, Francis A. TI Protons Sensitize Epithelial Cells to Mesenchymal Transition SO PLOS ONE LA English DT Article ID BETA ACTIVATION; MAMMARY-GLAND; STEM-CELLS; CANCER; GROWTH; PROGRESSION; EXPOSURE; RECEPTOR; THERAPY; TARGET AB Proton radiotherapy has gained more favor among oncologists as a treatment option for localized and deep-seated tumors. In addition, protons are a major constituent of the space radiation astronauts receive during space flights. The potential for these exposures to lead to, or enhance cancer risk has not been well studied. Our objective is to study the biological effects of low energy protons on epithelial cells and its propensity to enhance transforming growth factor beta 1 (TGF beta 1)-mediated epithelial-mesenchymal transition (EMT), a process occurring during tumor progression and critical for invasion and metastasis. Non-transformed mink lung epithelial cells (Mv1Lu) and hTERT-immortalized human esophageal epithelial cells (EPC) were used in this study. EMT was identified by alterations in cell morphology, EMT-related gene expression changes determined using real-time PCR, and EMT changes in specific cellular markers detected by immunostaining and western blotting. Although TGF beta 1 treatment alone is able to induce EMT in both Mv1Lu and EPC cells, low energy protons (5 MeV) at doses as low as 0.1 Gy can enhance TGF beta 1 induced EMT. Protons alone can also induce a mild induction of EMT. SD208, a potent TGF beta Receptor 1 (TGF beta R1) kinase inhibitor, can efficiently block TGF beta 1/Smad signaling and attenuate EMT induction. We suggest a model for EMT after proton irradiation in normal and cancerous tissue based on our results that showed that low and high doses of protons can sensitize normal human epithelial cells to mesenchymal transition, more prominently in the presence of TGF beta 1, but also in the absence of TGF beta 1. C1 [Wang, Minli; Hada, Megumi; Saha, Janapriya] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. [Sridharan, Deepa M.; Pluth, Janice M.] Lawrence Berkeley Natl Lab, Dept Canc & DNA Damage Responses, Berkeley, CA USA. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA. RP Wang, ML (reprint author), Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. EM francis.a.cucinotta@nasa.gov FU National Aeronautics and Space Administration; Department of Environment FX This work supported by National Aeronautics and Space Administration and Department of Environment. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 31 TC 9 Z9 10 U1 0 U2 2 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 23 PY 2012 VL 7 IS 7 AR e41249 DI 10.1371/journal.pone.0041249 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 977TM UT WOS:000306687700059 PM 22844446 ER PT J AU Hand, N Addison, GE Aubourg, E Battaglia, N Battistelli, ES Bizyaev, D Bond, JR Brewington, H Brinkmann, J Brown, BR Das, S Dawson, KS Devlin, MJ Dunkley, J Dunner, R Eisenstein, DJ Fowler, JW Gralla, MB Hajian, A Halpern, M Hilton, M Hincks, AD Hlozek, R Hughes, JP Infante, L Irwin, KD Kosowsky, A Lin, YT Malanushenko, E Malanushenko, V Marriage, TA Marsden, D Menanteau, F Moodley, K Niemack, MD Nolta, MR Oravetz, D Page, LA Palanque-Delabrouille, N Pan, K Reese, ED Schlegel, DJ Schneider, DP Sehgal, N Shelden, A Sievers, J Sifon, C Simmons, A Snedden, S Spergel, DN Staggs, ST Swetz, DS Switzer, ER Trac, H Weaver, BA Wollack, EJ Yeche, C Zunckel, C AF Hand, Nick Addison, Graeme E. Aubourg, Eric Battaglia, Nick Battistelli, Elia S. Bizyaev, Dmitry Bond, J. Richard Brewington, Howard Brinkmann, Jon Brown, Benjamin R. Das, Sudeep Dawson, Kyle S. Devlin, Mark J. Dunkley, Joanna Dunner, Rolando Eisenstein, Daniel J. Fowler, Joseph W. Gralla, Megan B. Hajian, Amir Halpern, Mark Hilton, Matt Hincks, Adam D. Hlozek, Renee Hughes, John P. Infante, Leopoldo Irwin, Kent D. Kosowsky, Arthur Lin, Yen-Ting Malanushenko, Elena Malanushenko, Viktor Marriage, Tobias A. Marsden, Danica Menanteau, Felipe Moodley, Kavilan Niemack, Michael D. Nolta, Michael R. Oravetz, Daniel Page, Lyman A. Palanque-Delabrouille, Nathalie Pan, Kaike Reese, Erik D. Schlegel, David J. Schneider, Donald P. Sehgal, Neelima Shelden, Alaina Sievers, Jon Sifon, Cristobal Simmons, Audrey Snedden, Stephanie Spergel, David N. Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Trac, Hy Weaver, Benjamin A. Wollack, Edward J. Yeche, Christophe Zunckel, Caroline TI Evidence of Galaxy Cluster Motions with the Kinematic Sunyaev-Zel'dovich Effect SO PHYSICAL REVIEW LETTERS LA English DT Article ID DIGITAL SKY SURVEY; SOUTH-POLE TELESCOPE; BULK FLOW; PECULIAR VELOCITIES; POWER SPECTRUM; DARK FLOW; COSMOLOGY; UNIVERSE; SYSTEMS; SAMPLE AB Using high-resolution microwave sky maps made by the Atacama Cosmology Telescope, we for the first time present strong evidence for motions of galaxy clusters and groups via microwave background temperature distortions due to the kinematic Sunyaev-Zel'dovich effect. Galaxy clusters are identified by their constituent luminous galaxies observed by the Baryon Oscillation Spectroscopic Survey, part of the Sloan Digital Sky Survey III. We measure the mean pairwise momentum of clusters, with a probability of the signal being due to random errors of 0.002, and the signal is consistent with the growth of cosmic structure in the standard model of cosmology. C1 [Hand, Nick] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hand, Nick; Hlozek, Renee; Sehgal, Neelima; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Addison, Graeme E.; Dunkley, Joanna] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Aubourg, Eric] Univ Paris Diderot, APC, Observ Paris, CNRS,IN2P3,CEA,IRFU, Sorbonne Paris Cite, France. [Battaglia, Nick; Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Bizyaev, Dmitry; Brewington, Howard; Brinkmann, Jon; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Shelden, Alaina; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA. [Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Nolta, Michael R.; Sievers, Jon; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Brown, Benjamin R.; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Das, Sudeep; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Dawson, Kyle S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Devlin, Mark J.; Reese, Erik D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Dunner, Rolando; Infante, Leopoldo; Sifon, Cristobal] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Eisenstein, Daniel J.] Harvard Coll Observ, Cambridge, MA 02138 USA. [Fowler, Joseph W.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Gralla, Megan B.; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Halpern, Mark] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Hincks, Adam D.; Page, Lyman A.; Sievers, Jon; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kosowsky, Arthur] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr, Pittsburgh, PA 15260 USA. [Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Moodley, Kavilan; Zunckel, Caroline] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Palanque-Delabrouille, Nathalie; Yeche, Christophe] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hand, N (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074; Sifon, Cristobal/0000-0002-8149-1352 FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768, OISE-0530095]; Berkeley Fellowship for Graduate Study; NSF [AST-0807790]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation under Compute Canada; Government of Ontario, Ontario Research Fund-Research Excellence; University of Toronto; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/NotreDame/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; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX This work was supported by the U.S. National Science Foundation through Grants AST-0408698 for the ACT project, and PHY-0355328, AST-0707731 and PIRE-0507768 (Grant number OISE-0530095). The PIRE program made possible exchanges between Chile, South Africa, Spain and the U.S. that enabled this research program. N. H. was partly supported by the Berkeley Fellowship for Graduate Study. A. K. was partly supported by NSF grant AST-0807790. Funding was also provided by Princeton University and the University of Pennsylvania. ACT mapmaking computation was performed on the GPC supercomputer at the SciNet HPC Consortium; SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund-Research Excellence, and the University of Toronto. ACT operates in the Chajnantor Science Preserve in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT). This work made use of the NASA Astrophysical Data System for bibliographic information. 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, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/NotreDame/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. We acknowledge Roman Juszkiewicz for pioneering work in the field of mean pairwise velocities. NR 47 TC 73 Z9 74 U1 1 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 23 PY 2012 VL 109 IS 4 AR 041101 DI 10.1103/PhysRevLett.109.041101 PG 6 WC Physics, Multidisciplinary SC Physics GA 977IY UT WOS:000306651900001 PM 23006072 ER PT J AU Meyers, VE Garcia, HD Monds, K Cooper, BL James, JT AF Meyers, Valerie E. Garcia, Hector D. Monds, Kathryn Cooper, Bonnie L. James, John T. TI Ocular toxicity of authentic lunar dust SO BMC OPHTHALMOLOGY LA English DT Article ID IRRITATION; SYMPTOMS; EYE AB Background: Dust exposure is a well-known occupational hazard for terrestrial workers and astronauts alike and will continue to be a concern as humankind pursues exploration and habitation of objects beyond Earth. Humankind's limited exploration experience with the Apollo Program indicates that exposure to dust will be unavoidable. Therefore, NASA must assess potential toxicity and recommend appropriate mitigation measures to ensure that explorers are adequately protected. Visual acuity is critical during exploration activities and operations aboard spacecraft. Therefore, the present research was performed to ascertain the ocular toxicity of authentic lunar dust. Methods: Small (mean particle diameter = 2.9 +/- 1.0 mu m), reactive lunar dust particles were produced by grinding bulk dust under ultrapure nitrogen conditions. Chemical reactivity and cytotoxicity testing were performed using the commercially available EpiOcular(TM) assay. Subsequent in vivo Draize testing utilized a larger size fraction of unground lunar dust that is more relevant to ocular exposures (particles <120 mu m; median particle diameter = 50.9 +/- 19.8 mu m). Results: In vitro testing indicated minimal irritancy potential based on the time required to reduce cell viability by 50% (ET50). Follow- up testing using the Draize standard protocol confirmed that the lunar dust was minimally irritating. Minor irritation of the upper eyelids was noted at the 1- hour observation point, but these effects resolved within 24 hours. In addition, no corneal scratching was observed using fluorescein stain. Conclusions: Low- titanium mare lunar dust is minimally irritating to the eyes and is considered a nuisance dust for ocular exposure. No special precautions are recommended to protect against ocular exposures, but fully shielded goggles may be used if dust becomes a nuisance. C1 [Meyers, Valerie E.; James, John T.] NASA, Lyndon B Johnson Space Ctr, Space Toxicol Off, Houston, TX 77058 USA. [Garcia, Hector D.] Wyle Sci Technol & Engn Grp, Space Toxicol Off, Houston, TX 77058 USA. [Monds, Kathryn] Stillmeadow Inc, Sugar Land, TX 77478 USA. [Cooper, Bonnie L.] Jacobs Technol, Houston, TX 77058 USA. RP James, JT (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Toxicol Off, 2101 NASA Pkwy,MC SF23, Houston, TX 77058 USA. EM john.t.james@nasa.gov FU NASA's Johnson Space Center; Wyle Bioastronautics Contract [NAS9-02078] FX This work was supported by NASA's Johnson Space Center and Wyle Bioastronautics Contract #NAS9-02078. Testing was performed by Stillmeadow, Inc., Sugarland, TX, under subcontract with Wyle's Science, Technology and Engineering Group. We thank Erica Trickey, Jocelyn Thomas, Paul Siemens, and Steven Balestrier of Stillmeadow, Inc. for their technical expertise and Sharon Barrow for her contribution as a technical writer for Stillmeadow, Inc. NR 13 TC 3 Z9 3 U1 3 U2 9 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2415 J9 BMC OPHTHALMOL JI BMC Ophthalmol. PD JUL 20 PY 2012 VL 12 AR 26 DI 10.1186/1471-2415-12-26 PG 7 WC Ophthalmology SC Ophthalmology GA 027QM UT WOS:000310368100001 PM 22817808 ER PT J AU Worden, HM Cheng, YF Pfister, G Carmichael, GR Zhang, Q Streets, DG Deeter, M Edwards, DP Gille, JC Worden, JR AF Worden, Helen M. Cheng, Yafang Pfister, Gabriele Carmichael, Gregory R. Zhang, Qiang Streets, David G. Deeter, Merritt Edwards, David P. Gille, John C. Worden, John R. TI Satellite-based estimates of reduced CO and CO2 emissions due to traffic restrictions during the 2008 Beijing Olympics SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CARBON-MONOXIDE; OZONE; MODEL AB During the 2008 Olympics, the Chinese government made a significant effort to improve air quality in Beijing, including restrictions on traffic. Here we estimate the reductions in carbon monoxide (CO) and carbon dioxide (CO2) emissions resulting from the control measures on Beijing transportation. Using MOPITT (Measurements Of Pollution In The Troposphere) multispectral satellite observations of near-surface CO along with WRF-Chem (Weather Research and Forecasting model with Chemistry) simulations for Beijing during August, 2007 and 2008, we estimate changes in CO due to meteorology and transportation sector emissions. Applying a reported CO/CO2 emission ratio for fossil fuels, we find the corresponding reduction in CO2, 60 +/- 36 Gg[CO2]/day. As compared to emission scenarios being considered for the IPCC AR5 (Intergovernmental Panel on Climate Change, 5th Assessment Report), this result suggests that urban traffic controls on the Beijing Olympics scale could play a significant role in meeting target reductions for global CO2 emissions. Citation: Worden, H.M., Y. Cheng, G. Pfister, G.R. Carmichael, Q. Zhang, D.G. Streets, M. Deeter, D.P. Edwards, J.C. Gille, and J.R. Worden (2012), Satellite-based estimates of reduced CO and CO2 emissions due to traffic restrictions during the 2008 Beijing Olympics, Geophys. Res. Lett., 39, L14802, doi:10.1029/2012GL052395. C1 [Worden, Helen M.; Pfister, Gabriele; Deeter, Merritt; Edwards, David P.; Gille, John C.] Natl Ctr Atmospher Res, Boulder, CO 80305 USA. [Cheng, Yafang; Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA USA. [Zhang, Qiang] Tsinghua Univ, Minist Educ, Key Lab Earth Syst Modeling, Beijing 100084, Peoples R China. [Zhang, Qiang] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China. [Streets, David G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Worden, John R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Worden, HM (reprint author), Natl Ctr Atmospher Res, 3450 Mitchell Ln, Boulder, CO 80305 USA. EM hmw@ucar.edu RI Cheng, Yafang/F-9362-2010; Pfister, Gabriele/A-9349-2008; Zhang, Qiang/D-9034-2012; Deeter, Merritt/O-6078-2016; OI Cheng, Yafang/0000-0003-4912-9879; Deeter, Merritt/0000-0002-3555-0518; Streets, David/0000-0002-0223-1350 FU Canadian Space Agency (CSA); Natural Sciences and Engineering Research Council (NSERC); Environment Canada; National Aeronautics and Space Administration (NASA) Earth Observing System (EOS) Program; National Science Foundation FX The authors thank Kevin Bowman, JPL/Cal-Tech, Dylan Jones, Univ. Toronto, Matthieu Pommier, Environment Canada, Louisa Emmons and J.-F. Lamarque, NCAR for their helpful suggestions. The MOPITT team also acknowledges the contributions of COMDEV (the prime contractor) and ABB BOMEM with support from the Canadian Space Agency (CSA), the Natural Sciences and Engineering Research Council (NSERC) and Environment Canada. The NCAR MOPITT project is supported by the National Aeronautics and Space Administration (NASA) Earth Observing System (EOS) Program. The National Center for Atmospheric Research (NCAR) is sponsored by the National Science Foundation. NR 29 TC 17 Z9 17 U1 4 U2 40 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 JUL 20 PY 2012 VL 39 AR L14802 DI 10.1029/2012GL052395 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 977YO UT WOS:000306701800001 ER PT J AU Mitrofanov, I Litvak, M Sanin, A Malakhov, A Golovin, D Boynton, W Droege, G Chin, G Evans, L Harshman, K Fedosov, F Garvin, J Kozyrev, A McClanahan, T Milikh, G Mokrousov, M Starr, R Sagdeev, R Shevchenko, V Shvetsov, V Tret'yakov, V Trombka, J Varenikov, A Vostrukhin, A AF Mitrofanov, I. Litvak, M. Sanin, A. Malakhov, A. Golovin, D. Boynton, W. Droege, G. Chin, G. Evans, L. Harshman, K. Fedosov, F. Garvin, J. Kozyrev, A. McClanahan, T. Milikh, G. Mokrousov, M. Starr, R. Sagdeev, R. Shevchenko, V. Shvetsov, V. Tret'yakov, V. Trombka, J. Varenikov, A. Vostrukhin, A. TI Testing polar spots of water-rich permafrost on the Moon: LEND observations onboard LRO SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LUNAR RECONNAISSANCE ORBITER; NEUTRON DETECTOR; NEAR-SURFACE; ICE DEPOSITS; MARS ODYSSEY; SOUTH-POLE; HYDROGEN; EMISSION; MERCURY; PLUME AB Results are presented for the LEND instrument onboard LRO for the detection of local spots of suppression and excess of epithermal neutron emission at the lunar poles. Twelve local Neutron Suppression Regions (NSRs) and Neutron Excess Regions (NERs) are detected. It is shown using the data from the LOLA and Diviner instruments that six NSRs have the empirical property "less local irradiation and lower temperature - fewer local neutrons." These NSRs may be identified with spots of water-ice rich permafrost on the Moon. It is shown that detected NSRs are include in both permanently shadowed and illuminated areas, and they are not coincident with Permanently Shadowed Regions (PSRs) at the bottom of polar craters, as has been commonly expected before LEND presented neutron data with high spatial resolution. C1 [Mitrofanov, I.; Litvak, M.; Sanin, A.; Malakhov, A.; Golovin, D.; Fedosov, F.; Kozyrev, A.; Mokrousov, M.; Tret'yakov, V.; Varenikov, A.; Vostrukhin, A.] Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. [Boynton, W.; Droege, G.; Harshman, K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Chin, G.; Garvin, J.; McClanahan, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Evans, L.] Comp Sci Corp, Greenbelt, MD USA. [Milikh, G.; Trombka, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Starr, R.] Catholic Univ, Dept Phys, Washington, DC USA. [Sagdeev, R.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Shevchenko, V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow, Russia. [Shvetsov, V.] Joint Inst Nucl Res, Dubna, Russia. RP Mitrofanov, I (reprint author), Russian Acad Sci, Inst Space Res, 84-32 Profsoyuznaya Str, Moscow 117997, Russia. EM imitrofa@space.ru FU International Space Science Institute FX This investigation was performed due to valuable support of all people of the LRO project, and authors are very much thankful to them for this excellent opportunity to study the Moon. The work for this paper was partially supported by grant for the research project "Nuclear Planetology" from the International Space Science Institute. The authors are also very much thankful to anonymous reviewers of this paper and to the Editor of the Journal of Geophysical Research-Planets for helpful comments and questions, which improved the paper. NR 41 TC 25 Z9 26 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUL 20 PY 2012 VL 117 AR E00H27 DI 10.1029/2011JE003956 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 977YH UT WOS:000306700900001 ER PT J AU Jennings, DE Anderson, CM Samuelson, RE Flasar, FM Nixon, CA Kunde, VG Achterberg, RK Cottini, V de Kok, R Coustenis, A Vinatier, S Calcutt, SB AF Jennings, Donald E. Anderson, C. M. Samuelson, R. E. Flasar, F. M. Nixon, C. A. Kunde, V. G. Achterberg, R. K. Cottini, V. de Kok, R. Coustenis, A. Vinatier, S. Calcutt, S. B. TI SEASONAL DISAPPEARANCE OF FAR-INFRARED HAZE IN TITAN'S STRATOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: individual (Titan); molecular processes; radiation mechanisms: thermal ID CASSINI; SPECTRA; ATMOSPHERE; TEMPERATURES; SPECTROMETER; UPDATE; SATURN; WINTER AB A far-infrared emission band attributed to volatile or refractory haze in Titan's stratosphere has been decreasing in intensity since Cassini's arrival in 2004. The 220 cm(-1) feature, first seen by the Voyager Infrared Interferometer Spectrometer, has only been found in Titan's winter polar region. The emission peaks at about 140 km altitude near the winter stratospheric temperature minimum. Observations recorded over the period 2004-2012 by the Composite Infrared Spectrometer on Cassini show a decrease in the intensity of this feature by about a factor of four. Possible seasonal causes of this decline are an increase in photolytic destruction of source chemicals at high altitude, a lessening of condensation as solar heating increased, or a weakening of downwelling of vapors. As of early 2012, the 220 cm(-1) haze has not yet been detected in the south. The haze composition is unknown, but its decrease is similar to that of HC3N gas in Titan's polar stratosphere, pointing to a nitrile origin. C1 [Jennings, Donald E.; Anderson, C. M.; Flasar, F. M.; Cottini, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Samuelson, R. E.; Nixon, C. A.; Kunde, V. G.; Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [de Kok, R.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Coustenis, A.; Vinatier, S.] Observ Paris, LESIA, F-92195 Meudon, France. [Calcutt, S. B.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. RP Jennings, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM donald.e.jennings@nasa.gov RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Anderson, Carrie/C-8097-2012; OI Nixon, Conor/0000-0001-9540-9121; Calcutt, Simon/0000-0002-0102-3170 FU NASA FX We acknowledge support from NASA's Cassini mission and Cassini Data Analysis Program. V.C. was supported by the NASA Postdoctoral Program. NR 34 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 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2012 VL 754 IS 1 AR L3 DI 10.1088/2041-8205/754/1/L3 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971XF UT WOS:000306238800003 ER PT J AU Kalapotharakos, C Harding, AK Kazanas, D Contopoulos, I AF Kalapotharakos, Constantinos Harding, Alice K. Kazanas, Demosthenes Contopoulos, Ioannis TI GAMMA-RAY LIGHT CURVES FROM PULSAR MAGNETOSPHERES WITH FINITE CONDUCTIVITY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: stars; pulsars: general; stars: neutron ID AREA TELESCOPE; SLOT GAPS; MAGNETIC-FIELD; VELA PULSAR; EMISSION; RADIATION; GEOMETRY; MODEL AB We investigate the shapes of gamma-ray pulsar light curves using three-dimensional pulsar magnetosphere models of finite conductivity. These models, covering the entire spectrum of solutions between vacuum and force-free magnetospheres, for the first time afford mapping the GeV emission of more realistic, dissipative pulsar magnetospheres. To this end we generate model light curves following two different approaches: (1) We employ the emission patterns of the slot and outer gap models in the field geometries of magnetospheres with different conductivity sigma. (2) We define realistic trajectories of radiating particles in magnetospheres of different sigma and compute their Lorentz factor under the influence of magnetospheric electric fields and curvature radiation-reaction; with these at hand we then calculate the emitted radiation intensity. The light curves resulting from these prescriptions are quite sensitive to the value of sigma, especially in the second approach. While still not self-consistent, these results are a step forward in understanding the physics of pulsar gamma-radiation. C1 [Kalapotharakos, Constantinos] Univ Maryland, Coll Pk UMDCP CRESST, College Pk, MD 20742 USA. [Kalapotharakos, Constantinos; Harding, Alice K.; Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Contopoulos, Ioannis] Acad Athens, Res Ctr Astron & Appl Math, Athens 11527, Greece. RP Kalapotharakos, C (reprint author), Univ Maryland, Coll Pk UMDCP CRESST, College Pk, MD 20742 USA. RI Harding, Alice/D-3160-2012 FU NASA Astrophysics Theory and Fundamental Physics Program; Fermi Guest Investigator Program FX A.K.H. acknowledges support from the NASA Astrophysics Theory and Fundamental Physics Program and the Fermi Guest Investigator Program. We also thank the referee for constructive comments. NR 27 TC 21 Z9 21 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 JUL 20 PY 2012 VL 754 IS 1 AR L1 DI 10.1088/2041-8205/754/1/L1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971XF UT WOS:000306238800001 ER PT J AU Katsuda, S Tsunemi, H Mori, K Uchida, H Petre, R Yamada, S Tamagawa, T AF Katsuda, Satoru Tsunemi, Hiroshi Mori, Koji Uchida, Hiroyuki Petre, Robert Yamada, Shin'ya Tamagawa, Toru TI DISCOVERY OF A PULSAR WIND NEBULA CANDIDATE IN THE CYGNUS LOOP SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (Cygnus Loop); ISM: supernova remnants; pulsars: general; stars: neutron; stars: winds, outflows; X-rays: ISM ID PHOTON IMAGING CAMERA; X-RAY; SUPERNOVA REMNANT; XMM-NEWTON; EINSTEIN OBSERVATIONS; SOUTHWESTERN RIM; PLASMA STRUCTURE; EMISSION; SUZAKU; CATALOG AB We report on a discovery of a diffuse nebula containing a pointlike source in the southern blowout region of the Cygnus Loop supernova remnant, based on Suzaku and XMM-Newton observations. The X-ray spectra from the nebula and the pointlike source are well represented by an absorbed power-law model with photon indices of 2.2 +/- 0.1 and 1.6 +/- 0.2, respectively. The photon indices as well as the flux ratio of F-nebula/F-pointlike similar to 4 lead us to propose that the system is a pulsar wind nebula, although pulsations have not yet been detected. If we attribute its origin to the Cygnus Loop supernova, then the 0.5-8 keV luminosity of the nebula is computed to be 2.1 x 10(31) (d/540 pc)(2) erg s(-1), where d is the distance to the Loop. This implies a spin-down loss-energy E. similar to 2.6 x 10(35) (d/540 pc)(2) erg s(-1). The location of the neutron star candidate, similar to 2 degrees away from the geometric center of the Loop, implies a high transverse velocity of similar to 1850 (theta/2 degrees) (d/540 pc) (t/10 kyr)(-1) km s(-1), assuming the currently accepted age of the Cygnus Loop. C1 [Katsuda, Satoru; Yamada, Shin'ya; Tamagawa, Toru] RIKEN Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Tsunemi, Hiroshi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 600043, Japan. [Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys & Elect Engn, Miyazaki 8892192, Japan. [Uchida, Hiroyuki] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Katsuda, S (reprint author), RIKEN Inst Phys & Chem Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. RI XRAY, SUZAKU/A-1808-2009 FU Special Postdoctoral Researchers Program in RIKEN; Ministry of Education, Culture, Sports, Science, and Technology [23000004]; MEXT [24740167] FX We thank Drs. Teruaki Enoto and Takao Kitaguchi for fruitful discussions. S.K. and S.Y. are supported by the Special Postdoctoral Researchers Program in RIKEN. This work is partly supported by a Grant-in-Aid for Scientific Research by the Ministry of Education, Culture, Sports, Science, and Technology (23000004). The work of K.M. is partially supported by the Grant-in-Aid for Young Scientists (B) of the MEXT (No. 24740167). NR 40 TC 2 Z9 2 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2012 VL 754 IS 1 AR L7 DI 10.1088/2041-8205/754/1/L7 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971XF UT WOS:000306238800007 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Decerprit, G Dickherber, R Duke, C Dumm, J Dwarkadas, VV Errando, M Falcone, A Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Huan, H Hughes, G Humensky, TB Kaaret, P Karlsson, N Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Lee, K Maier, G Majumdar, P McArthur, S McCann, A Millis, J Moriarty, P Mukherjee, R Nunez, PD Ong, RA Orr, M Otte, AN Pandel, D Park, N Perkins, JS Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Ruppel, J Saxon, DB Schroedter, M Sembroski, GH Skole, C Smith, AW Staszak, D Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Tyler, J Varlotta, A Vincent, S Vivier, M Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Welsing, R Williams, DA Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Decerprit, G. Dickherber, R. Duke, C. Dumm, J. Dwarkadas, V. V. Errando, M. Falcone, A. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Huan, H. Hughes, G. Humensky, T. B. Kaaret, P. Karlsson, N. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Lee, K. Maier, G. Majumdar, P. McArthur, S. McCann, A. Millis, J. Moriarty, P. Mukherjee, R. Nunez, P. D. Ong, R. A. Orr, M. Otte, A. N. Pandel, D. Park, N. Perkins, J. S. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Ruppel, J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Skole, C. Smith, A. W. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Tyler, J. Varlotta, A. Vincent, S. Vivier, M. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Welsing, R. Williams, D. A. Zitzer, B. TI VERITAS OBSERVATIONS OF THE NOVA IN V407 CYGNI SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; novae, cataclysmic variables; white dwarfs ID GAMMA-RAY EMISSION; RS-OPHIUCHI; CHERENKOV TELESCOPES; GALACTIC PLANE; 2006 OUTBURST; BLAST WAVE; DISCOVERY; ARRAY AB We report on very high energy (E > 100 GeV) gamma-ray observations of V407 Cygni, a symbiotic binary that underwent a nova outburst producing 0.1-10 GeV gamma rays during 2010 March 10-26. Observations were made with the Very Energetic Radiation Imaging Telescope Array System during 2010 March 19-26 at relatively large zenith angles due to the position of V407 Cyg. An improved reconstruction technique for large zenith angle observations is presented and used to analyze the data. We do not detect V407 Cygni and place a differential upper limit on the flux at 1.6 TeV of 2.3 x 10(-12) erg cm(-2) s(-1) (at the 95% confidence level). When considered jointly with data from Fermi-LAT, this result places limits on the acceleration of very high energy particles in the nova. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Majumdar, P.; Ong, R. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Collins-Hughes, E.; Khassen, Y.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Connolly, M. P.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Decerprit, G.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Skole, C.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Kieda, D.; Nunez, P. D.; Smith, A. W.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Huan, H.; Park, N.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Krennrich, F.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Perkins, J. S.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Aliu, E (reprint author), Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. EM daniel-d-gall@uiowa.edu; kazuma-tsurusaki@uiowa.edu RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK FX We thank Pierre Jean of the Fermi-LAT team for providing the contour data from the Fermi-LAT results and useful discussion. This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution; by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748); and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 36 TC 13 Z9 13 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 JUL 20 PY 2012 VL 754 IS 1 AR 77 DI 10.1088/0004-637X/754/1/77 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800077 ER PT J AU Bachelet, E Shin, IG Han, C Fouque, P Gould, A Menzies, JW Beaulieu, JP Bennett, DP Bond, IA Dong, S Heyrovsky, D Marquette, JB Marshall, J Skowron, J Street, RA Sumi, T Udalski, A Abe, L Agabi, K Albrow, MD Allen, W Bertin, E Bos, M Bramich, DM Chavez, J Christie, GW Cole, AA Crouzet, N Dieters, S Dominik, M Drummond, J Greenhill, J Guillot, T Henderson, CB Hessman, FV Horne, K Hundertmark, M Johnson, JA Jorgensen, UG Kandori, R Liebig, C Mekarnia, D McCormick, J Moorhouse, D Nagayama, T Nataf, D Natusch, T Nishiyama, S Rivet, JP Sahu, KC Shvartzvald, Y Thornley, G Tomczak, AR Tsapras, Y Yee, JC Batista, V Bennett, CS Brillant, S Caldwell, JAR Cassan, A Corrales, E Coutures, C Prester, DD Donatowicz, J Kubas, D Martin, R Williams, A Zub, M de Almeida, LA DePoy, DL Gaudi, BS Hung, LW Jablonski, F Kaspi, S Klein, N Lee, CU Lee, Y Koo, JR Maoz, D Munoz, JA Pogge, RW Polishook, D Shporer, A Abe, F Botzler, CS Chote, P Freeman, M Fukui, A Furusawa, K Harris, P Itow, Y Kobara, S Ling, CH Masuda, K Matsubara, Y Miyake, N Ohmori, K Ohnishi, K Rattenbury, NJ Saito, T Sullivan, DJ Suzuki, D Sweatman, WL Tristram, PJ Wada, K Yock, PCM Szymanski, MK Soszynski, I Kubiak, M Poleski, R Ulaczyk, K Pietrzynski, G Wyrzykowski, L Kains, N Snodgrass, C Steele, IA Alsubai, KA Bozza, V Browne, P Burgdorf, MJ Novati, SC Dodds, P Dreizler, S Finet, F Gerner, T Hardis, S Harpsoe, K Hinse, TC Kerins, E Mancini, L Mathiasen, M Penny, MT Proft, S Rahvar, S Ricci, D Scarpetta, G Schafer, S Schonebeck, F Southworth, J Surdej, J Wambsganss, J AF Bachelet, E. Shin, I. -G. Han, C. Fouque, P. Gould, A. Menzies, J. W. Beaulieu, J. -P. Bennett, D. P. Bond, I. A. Dong, Subo Heyrovsky, D. Marquette, J. -B. Marshall, J. Skowron, J. Street, R. A. Sumi, T. Udalski, A. Abe, L. Agabi, K. Albrow, M. D. Allen, W. Bertin, E. Bos, M. Bramich, D. M. Chavez, J. Christie, G. W. Cole, A. A. Crouzet, N. Dieters, S. Dominik, M. Drummond, J. Greenhill, J. Guillot, T. Henderson, C. B. Hessman, F. V. Horne, K. Hundertmark, M. Johnson, J. A. Jorgensen, U. G. Kandori, R. Liebig, C. Mekarnia, D. McCormick, J. Moorhouse, D. Nagayama, T. Nataf, D. Natusch, T. Nishiyama, S. Rivet, J. -P. Sahu, K. C. Shvartzvald, Y. Thornley, G. Tomczak, A. R. Tsapras, Y. Yee, J. C. Batista, V. Bennett, C. S. Brillant, S. Caldwell, J. A. R. Cassan, A. Corrales, E. Coutures, C. Prester, D. Dominis Donatowicz, J. Kubas, D. Martin, R. Williams, A. Zub, M. Andrade de Almeida, L. DePoy, D. L. Gaudi, B. S. Hung, L. -W. Jablonski, F. Kaspi, S. Klein, N. Lee, C. -U. Lee, Y. Koo, J. -R. Maoz, D. Munoz, J. A. Pogge, R. W. Polishook, D. Shporer, A. Abe, F. Botzler, C. S. Chote, P. Freeman, M. Fukui, A. Furusawa, K. Harris, P. Itow, Y. Kobara, S. Ling, C. H. Masuda, K. Matsubara, Y. Miyake, N. Ohmori, K. Ohnishi, K. Rattenbury, N. J. Saito, To. Sullivan, D. J. Suzuki, D. Sweatman, W. L. Tristram, P. J. Wada, K. Yock, P. C. M. Szymanski, M. K. Soszynski, I. Kubiak, M. Poleski, R. Ulaczyk, K. Pietrzynski, G. Wyrzykowski, L. Kains, N. Snodgrass, C. Steele, I. A. Alsubai, K. A. Bozza, V. Browne, P. Burgdorf, M. J. Novati, S. Calchi Dodds, P. Dreizler, S. Finet, F. Gerner, T. Hardis, S. Harpsoe, K. Hinse, T. C. Kerins, E. Mancini, L. Mathiasen, M. Penny, M. T. Proft, S. Rahvar, S. Ricci, D. Scarpetta, G. Schaefer, S. Schoenebeck, F. Southworth, J. Surdej, J. Wambsganss, J. CA PLANET Collaboration FUN Collaboration MOA Collaboration OGLE Collaboration RoboNet Collaboration MiNDSTEp Consortium TI MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems ID DIFFERENCE IMAGE-ANALYSIS; HIGH-MAGNIFICATION; GALACTIC BULGE; SNOW LINE; JUPITER/SATURN ANALOG; PROTOPLANETARY DISK; MILKY-WAY; EVENTS; BINARY; STARS AB Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 +/- 0.004) x 10(-3) and the projected separation is s = 1.1228 +/- 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large theta(E) = 1.38 +/- 0.11 mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range 0.13 < M/M-circle dot < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M-* = 0.67(-0.13)(+0.33) M-circle dot and m(p) = 1.5(-0.3)(+0.8) M-JUP at a distance of D = 2.3 +/- 0.6 kpc, and with a semi-major axis of a = 2(-1)(+3) AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric. C1 [Shin, I. -G.; Han, C.] Chungbuk Natl Univ, Dept Phys, Chonju 361763, South Korea. [Bachelet, E.; Fouque, P.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France. [Gould, A.; Dong, Subo; Marshall, J.; Skowron, J.; Henderson, C. B.; Johnson, J. A.; Nataf, D.; Yee, J. C.; Batista, V.; Gaudi, B. S.; Hung, L. -W.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Menzies, J. W.] S African Astron Observ, ZA-7925 Observatory, South Africa. [Beaulieu, J. -P.; Marquette, J. -B.; Bertin, E.; Batista, V.; Cassan, A.; Corrales, E.; Coutures, C.; Kubas, D.] UPMC, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, Auckland 1330, New Zealand. [Dong, Subo] Inst Adv Study, Princeton, NJ 08540 USA. [Heyrovsky, D.] Charles Univ Prague, Inst Theoret Phys, CR-18000 Prague, Czech Republic. [Street, R. A.; Tsapras, Y.; Shporer, A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Sumi, T.; Abe, F.; Furusawa, K.; Itow, Y.; Kobara, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Ohmori, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Udalski, A.; Szymanski, M. K.; Soszynski, I.; Kubiak, M.; Poleski, R.; Ulaczyk, K.; Pietrzynski, G.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Abe, L.; Agabi, K.; Crouzet, N.; Guillot, T.; Mekarnia, D.; Rivet, J. -P.] Observ Cote Azur, Lab Fizeau, F-06300 Nice, France. [Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Allen, W.] Vintage Lane Observ, Blenheim, New Zealand. [Bos, M.] Molehill Astron Observ, N Shore, New Zealand. [Bramich, D. M.; Kains, N.] European So Observ, D-85748 Garching, Germany. [Chavez, J.; Caldwell, J. A. R.] McDonald Observ, Ft Davis, TX 79734 USA. [Christie, G. W.; Natusch, T.] Auckland Observ, Auckland, New Zealand. [Cole, A. A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Dominik, M.; Horne, K.; Hundertmark, M.; Liebig, C.; Kains, N.; Browne, P.; Dodds, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Drummond, J.] Possum Observ, John Drummond, New Zealand. [Hessman, F. V.; Hundertmark, M.; Dreizler, S.; Schaefer, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Jorgensen, U. G.; Hardis, S.; Harpsoe, K.; Mathiasen, M.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, U. G.; Harpsoe, K.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen O, Denmark. [Kandori, R.] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. [Liebig, C.; Zub, M.; Gerner, T.; Proft, S.; Schoenebeck, F.; Wambsganss, J.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand. [Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand. [Nagayama, T.] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Natusch, T.] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand. [Nishiyama, S.] Natl Inst Nat Sci, Natl Astron Observ Japan, Extrasolar Planet Detect Project Off, Mitaka, Tokyo 1818588, Japan. [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Shvartzvald, Y.; Kaspi, S.; Klein, N.; Maoz, D.; Polishook, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Shvartzvald, Y.; Kaspi, S.; Klein, N.; Maoz, D.; Polishook, D.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. [Tomczak, A. R.; DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Bennett, C. S.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Brillant, S.; Kubas, D.] European So Observ, Santiago 19, Chile. [Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia. [Donatowicz, J.] Vienna Univ Technol, A-1040 Vienna, Austria. [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia. [Andrade de Almeida, L.; Jablonski, F.] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Lee, C. -U.; Koo, J. -R.; Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Lee, Y.] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon, South Korea. [Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. [Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Chote, P.; Harris, P.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Fukui, A.] Natl Astron Observ, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Alsubai, K. A.] Qatar Fdn, Doha, Qatar. [Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84081 Baronissi, SA, Italy. [Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. [Burgdorf, M. J.] NASA Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Novati, S. Calchi] IIASS, Vietri Sul Mare, SA, Italy. [Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Kerins, E.; Penny, M. T.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Mancini, L.] Max Planck Inst Astron, D-619117 Heidelberg, Germany. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran. [Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, Grp Collegato Salerno, Naples, Italy. [Southworth, J.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, Chonju 361763, South Korea. RI Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; Almeida, L./G-7188-2012; Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012; Greenhill, John/C-8367-2013; 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Williams, Andrew/K-2931-2013; Skowron, Jan/M-5186-2014; Heyrovsky, David/A-2031-2015 OI Cole, Andrew/0000-0003-0303-3855; Ricci, Davide/0000-0002-9790-0552; Penny, Matthew/0000-0001-7506-5640; Snodgrass, Colin/0000-0001-9328-2905; Hundertmark, Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Williams, Andrew/0000-0001-9080-0105; Skowron, Jan/0000-0002-2335-1730; Heyrovsky, David/0000-0002-5198-5343 FU National Research Foundation of Korea [2009-0081561]; MOA [JSPS20340052, JSPS22403003]; Czech Science Foundation [GACR P209/10/1318]; French Polar Institute (IPEV); European Research Council under the European Community's Seventh Framework Programme/ERC [246678]; CALMIP [2011-P1131]; NSF [AST-1103471, 2009068160]; NASA [NNG04GL51G]; KRCF Young Scientist Research Fellowship Program in South Korea; ANR; CNRS; Observatoire de la Cote d'Azur; California Institute of Technology (Caltech); NASA; ANR HOLMES; ANR PNPS FX We acknowledge the following sources of support: the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea (C.H.); grants JSPS20340052 and JSPS22403003 for MOA; Czech Science Foundation grant GACR P209/10/1318; the French Polar Institute (IPEV) and the Italian Antarctic Programme (PNRA) for the logistics and data transmission at Concordia. OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678. Part of the computer work was performed using HPC resources from CALMIP (Grant 2011-P1131).; E. Bachelet gratefully acknowledges the Chungbuk National University for a one-month stay where most of this work was prepared. B. S. Gaudi and A. Gould acknowledge support from NSF AST-1103471. B. S. Gaudi, A. Gould, and R. W. Pogge acknowledge support from the NASA grant NNG04GL51G. Work by J. C. Yee is supported by the National Science Foundation Graduate Research Fellowship under grant No. 2009068160. T. C. Hinse acknowledges support from the KRCF Young Scientist Research Fellowship Program in South Korea. The PLANET collaboration acknowledges the financial support of ANR HOLMES and PNPS grants. ASTEP was financed through the help of ANR, IPEV, CNRS, Observatoire de la Cote d'Azur. Work by S. D. was performed under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. NR 80 TC 22 Z9 22 U1 1 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2012 VL 754 IS 1 AR 73 DI 10.1088/0004-637X/754/1/73 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800073 ER PT J AU Brosius, JW AF Brosius, Jeffrey W. TI EXTREME-ULTRAVIOLET SPECTROSCOPIC OBSERVATION OF DIRECT CORONAL HEATING DURING A C-CLASS SOLAR FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: flares; Sun: transition region; Sun: UV radiation; Sun: X-rays, gamma rays ID LOOP RADIATIVE HYDRODYNAMICS; HIGH TIME RESOLUTION; CHROMOSPHERIC EVAPORATION; DIAGNOSTIC SPECTROMETER; MAGNETIC RECONNECTION; ENERGY-TRANSPORT; SOHOS CDS; RHESSI; MICROFLARE; EVOLUTION AB With the Coronal Diagnostic Spectrometer operating in rapid cadence (9.8 s) stare mode during a C6.6 flare on the solar disk, we observed a sudden brightening of Fe XIX line emission (formed at temperature T approximate to 8 MK) above the pre-flare noise without a corresponding brightening of emission from ions formed at lower temperatures, including He I (0.01 MK), O V (0.25 MK), and Si XII (2 MK). The sudden brightening persisted as a plateau of Fe XIX intensity that endured more than 11 minutes. The Fe XIX emission at the rise and during the life of the plateau showed no evidence of significant bulk velocity flows, and hence cannot be attributed to chromospheric evaporation. However, the line width showed a significant broadening at the rise of the plateau, corresponding to nonthermal velocities of at least 89 km s(-1) due to reconnection outflows or turbulence. During the plateau He I, O V, and Si XII brightened at successively later times starting about 3.5 minutes after Fe XIX, which suggests that these brightenings were produced by thermal conduction from the plasma that produced the Fe XIX line emission; however, we cannot rule out the possibility that they were produced by a weak beam of nonthermal particles. We interpret an observed shortening of the O V wavelength for about 1.5 minutes toward the middle of the plateau to indicate new upward motions driven by the flare, as occurs during gentle chromospheric evaporation; relative to a quiescent interval shortly before the flare, the O V upward velocity was around -10 km s(-1). C1 NASA, Goddard Space Flight Ctr, Solar Phys Lab, Catholic Univ Amer, Greenbelt, MD 20771 USA. RP Brosius, JW (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Catholic Univ Amer, Code 671, Greenbelt, MD 20771 USA. EM Jeffrey.W.Brosius@nasa.gov FU NASA [NNX10AC08G] FX J.W.B. acknowledges NASA support through SR&T grant NNX10AC08G. NR 39 TC 8 Z9 8 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 JUL 20 PY 2012 VL 754 IS 1 AR 54 DI 10.1088/0004-637X/754/1/54 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800054 ER PT J AU Camero-Arranz, A Finger, MH Wilson-Hodge, CA Jenke, P Steele, I Coe, MJ Gutierrez-Soto, J Kretschmar, P Caballero, I Yan, J Rodriguez, J Suso, J Case, G Cherry, ML Guiriec, S McBride, VA AF Camero-Arranz, A. Finger, M. H. Wilson-Hodge, C. A. Jenke, P. Steele, I. Coe, M. J. Gutierrez-Soto, J. Kretschmar, P. Caballero, I. Yan, J. Rodriguez, J. Suso, J. Case, G. Cherry, M. L. Guiriec, S. McBride, V. A. TI X-RAY AND OPTICAL OBSERVATIONS OF A 0535+26 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars: individual (A 0535+26); stars: emission-line, Be; stars: neutron; X-rays: binaries ID QUASI-PERIODIC OSCILLATIONS; AUGUST/SEPTEMBER 2005 OUTBURST; PULSAR SAX J1808.4-3658; BINARY 1A 0535+262; EQUATION-OF-STATE; MILLISECOND PULSAR; TIMING EXPLORER; BURST MONITOR; ACCRETION TORQUES; GIANT OUTBURST AB We present recent contemporaneous X-ray and optical observations of the Be/X-ray binary system A 0535+26 with the Fermi/Gamma-ray Burst Monitor (GBM) and several ground-based observatories. These new observations are put into the context of the rich historical data (since similar to 1978) and discussed in terms of the neutron-star-Be-disk interaction. The Be circumstellar disk was exceptionally large just before the 2009 December giant outburst, which may explain the origin of the unusual recent X-ray activity of this source. We found a peculiar evolution of the pulse profile during this giant outburst, with the two main components evolving in opposite ways with energy. A hard 30-70 mHz X-ray quasi-periodic oscillation was detected with GBM during this 2009 December giant outburst. It becomes stronger with increasing energy and disappears at energies below 25 keV. In the long term a strong optical/X-ray correlation was found for this system, however in the medium term the H alpha equivalent width and the V-band brightness showed an anti-correlation after similar to 2002 August. Each giant X-ray outburst occurred during a decline phase of the optical brightness, while the H alpha showed a strong emission. In late 2010 and before the 2011 February outburst, rapid V/R variations are observed in the strength of the two peaks of the H alpha line. These had a period of similar to 25 days and we suggest the presence of a global one-armed oscillation to explain this scenario. A general pattern might be inferred, where the disk becomes weaker and shows V/R variability beginning similar to 6 months following a giant outburst. C1 [Camero-Arranz, A.; Finger, M. H.] Univ Space Res Assoc, Huntsville, AL 35806 USA. [Camero-Arranz, A.; Finger, M. H.; Wilson-Hodge, C. A.; Jenke, P.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Steele, I.] Liverpool John Moores Univ, Liverpool L3 2AJ, Merseyside, England. [Coe, M. J.; McBride, V. A.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Gutierrez-Soto, J.] Inst Astrofis Andalucia, E-18008 Granada, Spain. [Gutierrez-Soto, J.] Valencian Int Univ, Castellon De La Plana 12006, Spain. [Kretschmar, P.] ESA ESAC, Madrid, Spain. [Caballero, I.; Rodriguez, J.] AIM CEA Saclay, Paris, France. [Yan, J.] Chinese Acad Sci, Purple Mt Observ, Beijing, Peoples R China. [Suso, J.] Univ Valencia, Paterna 46980, Spain. [Case, G.; Cherry, M. L.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Guiriec, S.] NASA GSFC, Greenbelt, MD 20771 USA. RP Camero-Arranz, A (reprint author), Univ Space Res Assoc, Huntsville, AL 35806 USA. RI Gutierrez-Soto, Juan/H-9620-2015; Suso , Julia/F-8076-2016; OI Gutierrez-Soto, Juan/0000-0001-6736-0551; Kretschmar, Peter/0000-0001-9840-2048; Rodriguez, Jerome/0000-0002-4151-4468 FU NASA [NNX08AW06G, NNX11AE24G]; NASA Postdoctoral Program at NASA Marshall Space Flight Center FX A.C.A. and M.H.F. acknowledge support from NASA grants NNX08AW06G and NNX11AE24G. P.J. acknowledges support from NASA Postdoctoral Program at NASA Marshall Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. J.G.S. acknowledges the Instituto de Astrofisica de Andalucia (CSIC) for allowing us to access to the 0.9 and 1.5 m telescopes at the OSN at the Observatorio de Sierra Nevada (Spain). A. C. A thanks to Alessandro Pappito for providing very useful information on millisecond accreting X-ray pulsars. We thank to all the Fermi/GBM Occultation team for its help and in general to all the GBM team based in Huntsville, Alabama. NR 94 TC 12 Z9 12 U1 1 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 JUL 20 PY 2012 VL 754 IS 1 AR 20 DI 10.1088/0004-637X/754/1/20 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800020 ER PT J AU Frye, BL Hurley, M Bowen, DV Meurer, G Sharon, K Straughn, A Coe, D Broadhurst, T Guhathakurta, P AF Frye, Brenda L. Hurley, Mairead Bowen, David V. Meurer, Gerhardt Sharon, Keren Straughn, Amber Coe, Dan Broadhurst, Tom Guhathakurta, Puragra TI SPATIALLY RESOLVED HST GRISM SPECTROSCOPY OF A LENSED EMISSION LINE GALAXY AT z similar to 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: individual (A1689); galaxies: distances and redshifts; galaxies: fundamental parameters ID STAR-FORMING GALAXIES; ULTRA DEEP FIELD; MASS-METALLICITY RELATION; DIGITAL SKY SURVEY; EXTRAGALACTIC LEGACY SURVEY; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; PHYSICAL CONDITIONS; ADVANCED CAMERA AB We take advantage of gravitational lensing amplification by A1689 (z = 0.187) to undertake the first space-based census of emission line galaxies (ELGs) in the field of a massive lensing cluster. Forty-three ELGs are identified to a flux of i(775) = 27.3 via slitless grism spectroscopy. One ELG (at z = 0.7895) is very bright owing to lensing magnification by a factor of approximate to 4.5. Several Balmer emission lines (ELs) detected from ground-based follow-up spectroscopy signal the onset of a major starburst for this low-mass galaxy (M-* approximate to 2 x 10(9) M-circle dot) with a high specific star formation rate (approximate to 20 Gyr(-1)). From the blue ELs we measure a gas-phase oxygen abundance consistent with solar (12+log(O/H) = 8.8+/-0.2). We break the continuous line-emitting region of this giant arc into seven similar to 1 kpc bins (intrinsic size) and measure a variety of metallicity-dependent line ratios. A weak trend of increasing metal fraction is seen toward the dynamical center of the galaxy. Interestingly, the metal line ratios in a region offset from the center by similar to 1 kpc have a placement on the blue H II region excitation diagram with f([O III])/f(H beta) and f ([Ne III])/f(H beta) that can be fitted by an active galactic nucleus (AGN). This asymmetrical AGN-like behavior is interpreted as a product of shocks in the direction of the galaxy's extended tail, possibly instigated by a recent galaxy interaction. C1 [Frye, Brenda L.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Frye, Brenda L.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Frye, Brenda L.] Univ San Francisco, Dept Phys & Astrophys, San Francisco, CA 94117 USA. [Hurley, Mairead] Dublin City Univ, Sch Phys Sci, Dublin 9, Ireland. [Bowen, David V.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08540 USA. [Meurer, Gerhardt] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Sharon, Keren] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Straughn, Amber] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Coe, Dan] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Broadhurst, Tom] Ikerbasque, E-48011 Bilbao, Spain. [Guhathakurta, Puragra] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Frye, BL (reprint author), Univ Arizona, Dept Astron, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM bfrye@as.arizona.edu FU W. M. Keck Foundation; NASA [NAS 5-32865, NAG5-7697]; Sun Microsystems, Inc.; NASA Long-Term Space Astrophysics [NNG05GE26G] FX Based, in part, on data obtained with the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation.; ACS. was developed under NASA contract NAS 5-32865, and this research has been supported in part by NASA grant NAG5-7697 and by an equipment grant from Sun Microsystems, Inc. B. L. F. acknowledges generous hospitality at the SUNY Stony Brook Astronomy Group. D. V. B. is funded through NASA Long-Term Space Astrophysics grant NNG05GE26G. We are grateful to Sangeeta Malhotra and James Rhoads for providing useful follow-up spectroscopy on Magellan Observatories. We thank Holland Ford, Rogier Windhorst, Nicole Nesvadba, Jean-Paul Kneib, and Marusa Bradac for useful discussions. Some data for this work were acquired at Keck Observatories. We also want to express our appreciation to the anonymous referee whose comments and suggestions improved the clarity of this paper. The authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, some of the observations presented herein would not have been possible. NR 89 TC 9 Z9 9 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 JUL 20 PY 2012 VL 754 IS 1 AR 17 DI 10.1088/0004-637X/754/1/17 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800017 ER PT J AU Fuselier, SA Allegrini, F Bzowski, M Funsten, HO Ghielmetti, AG Gloeckler, G Heirtzler, D Janzen, P Kubiak, M Kucharek, H McComas, DJ Mobius, E Moore, TE Petrinec, SM Quinn, M Reisenfeld, D Saul, LA Scheer, JA Schwadron, N Trattner, KJ Vanderspek, R Wurz, P AF Fuselier, S. A. Allegrini, F. Bzowski, M. Funsten, H. O. Ghielmetti, A. G. Gloeckler, G. Heirtzler, D. Janzen, P. Kubiak, M. Kucharek, H. McComas, D. J. Moebius, E. Moore, T. E. Petrinec, S. M. Quinn, M. Reisenfeld, D. Saul, L. A. Scheer, J. A. Schwadron, N. Trattner, K. J. Vanderspek, R. Wurz, P. TI HELIOSPHERIC NEUTRAL ATOM SPECTRA BETWEEN 0.01 AND 6 keV FROM IBEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE interplanetary medium; ISM: molecules; plasmas; solar wind; Sun: heliosphere ID INTERSTELLAR BOUNDARY EXPLORER; INNER HELIOSHEATH; HYDROGEN-ATOMS; CASSINI; RIBBON; FLUX AB Since 2008 December, the Interstellar Boundary Explorer (IBEX) has been making detailed observations of neutrals from the boundaries of the heliosphere using two neutral atom cameras with overlapping energy ranges. The unexpected, yet defining feature discovered by IBEX is a Ribbon that extends over the energy range from about 0.2 to 6 keV. This Ribbon is superposed on a more uniform, globally distributed heliospheric neutral population. With some important exceptions, the focus of early IBEX studies has been on neutral atoms with energies greater than similar to 0.5 keV. With nearly three years of science observations, enough low-energy neutral atom measurements have been accumulated to extend IBEX observations to energies less than similar to 0.5 keV. Using the energy overlap of the sensors to identify and remove backgrounds, energy spectra over the entire IBEX energy range are produced. However, contributions by interstellar neutrals to the energy spectrum below 0.2 keV may not be completely removed. Compared with spectra at higher energies, neutral atom spectra at lower energies do not vary much from location to location in the sky, including in the direction of the IBEX Ribbon. Neutral fluxes are used to show that low energy ions contribute approximately the same thermal pressure as higher energy ions in the heliosheath. However, contributions to the dynamic pressure are very high unless there is, for example, turbulence in the heliosheath with fluctuations of the order of 50-100 km s(-1). C1 [Fuselier, S. A.; Ghielmetti, A. G.; Petrinec, S. M.; Trattner, K. J.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. [Fuselier, S. A.; Allegrini, F.; McComas, D. J.] SW Res Inst, San Antonio, TX 78228 USA. [Allegrini, F.; McComas, D. J.] Univ Texas San Antonio, San Antonio, TX 78249 USA. [Bzowski, M.; Kubiak, M.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland. [Funsten, H. O.; Moebius, E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Gloeckler, G.] Univ Michigan, Ann Arbor, MI 48109 USA. [Heirtzler, D.; Kucharek, H.; Moebius, E.; Quinn, M.; Schwadron, N.] Univ New Hampshire, Durham, NH 03824 USA. [Janzen, P.; Reisenfeld, D.] Univ Montana, Missoula, MT 59812 USA. [Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Saul, L. A.; Scheer, J. A.; Wurz, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Vanderspek, R.] MIT, Cambridge, MA 02139 USA. RP Fuselier, SA (reprint author), Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. EM sfuselier@swri.edu; fallegrini@swri.edu; bzowski@cbk.waw.pl; hfunsten@lanl.gov; gmetti_elopt@gmx.ch; gglo@umich.edu; paul.janzen@umontana.edu; mkubiak@cbk.waw.pl; harald.kucharek@unh.edu; dmccomas@swri.edu; eberhard.moebius@unh.edu; Thomas.Moore@nasa.gov; steven.m.petrinec@lmco.com; marty@drsri.com; dan.reisenfeld@umontana.edu; luke.saul@gmail.com; juergen.scheer@space.unibe.ch; n.schwadron@unh.edu; Karlheinz.J.Trattner@lmco.com; roland@space.mit.edu; peter.wurz@space.unibe.ch RI Moore, Thomas/D-4675-2012; Funsten, Herbert/A-5702-2015; Reisenfeld, Daniel/F-7614-2015; OI Moore, Thomas/0000-0002-3150-1137; Funsten, Herbert/0000-0002-6817-1039; Moebius, Eberhard/0000-0002-2745-6978 FU NASA FX Support for this study comes from NASA's Explorer program. IBEX is the result of efforts from a large number of scientists, engineers, and others. All who contributed to this mission share in its success. NR 31 TC 23 Z9 23 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2012 VL 754 IS 1 AR 14 DI 10.1088/0004-637X/754/1/14 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800014 ER PT J AU Hamaguchi, K Grosso, N Kastner, JH Weintraub, DA Richmond, M Petre, R Teets, WK Principe, D AF Hamaguchi, Kenji Grosso, Nicolas Kastner, Joel H. Weintraub, David A. Richmond, Michael Petre, Robert Teets, William K. Principe, David TI X-RAYING THE BEATING HEART OF A NEWBORN STAR: ROTATIONAL MODULATION OF HIGH-ENERGY RADIATION FROM V1647 Ori SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; stars: individual (V1647 Ori); stars: pre-main sequence; X-rays: stars ID ACCRETING YOUNG STAR; T-TAURI; FU ORIONIS; MAGNETIC-FIELD; OUTBURST; EMISSION; FLARES; NEBULA; DISK; EVOLUTION AB We report a periodicity of similar to 1 day in the highly elevated X-ray emission from the protostar V1647 Ori during its two recent multiple-year outbursts of mass accretion. This periodicity is indicative of protostellar rotation at near-break-up speed. Modeling of the phased X-ray light curve indicates that the high-temperature (similar to 50 MK), X-ray-emitting plasma, which is most likely heated by accretion-induced magnetic reconnection, resides in dense (greater than or similar to 5 x 10(10) cm(-3)), pancake-shaped magnetic footprints where the accretion stream feeds the newborn star. The sustained X-ray periodicity of V1647 Ori demonstrates that such protostellar magnetospheric accretion configurations can be stable over timescales of years. C1 [Hamaguchi, Kenji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Hamaguchi, Kenji; Petre, Robert] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Hamaguchi, Kenji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Grosso, Nicolas] Univ Strasbourg, CNRS, UMR 7550, Observ Astron Strasbourg, F-67000 Strasbourg, France. [Kastner, Joel H.; Richmond, Michael; Principe, David] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Weintraub, David A.; Teets, William K.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. RP Hamaguchi, K (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. EM Kenji.Hamaguchi@nasa.gov FU NASA's Astrobiology Institute [RTOP 344-53-51]; NASA/GSFC XMM-Newton Guest Observer [NNX09AC11G] FX This work is performed while K.H. was supported by the NASA's Astrobiology Institute (RTOP 344-53-51) to the Goddard Center for Astrobiology (Michael J. Mumma, P. I.). J.K.'s research on X-rays from erupting YSOs is supported by NASA/GSFC XMM-Newton Guest Observer grant NNX09AC11G to RIT. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. NR 39 TC 11 Z9 11 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 JUL 20 PY 2012 VL 754 IS 1 AR 32 DI 10.1088/0004-637X/754/1/32 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800032 ER PT J AU Krick, JE Glaccum, WJ Carey, SJ Lowrance, PJ Surace, JA Ingalls, JG Hora, JL Reach, WT AF Krick, Jessica E. Glaccum, William J. Carey, Sean J. Lowrance, Patrick J. Surace, Jason A. Ingalls, James G. Hora, Joseph L. Reach, William T. TI A SPITZER/IRAC MEASURE OF THE ZODIACAL LIGHT SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; infrared: diffuse background; interplanetary medium ID BACKGROUND EXPERIMENT SEARCH; THERMAL EMISSION; SPACE-TELESCOPE; DUST CLOUD; COBE; DIRBE; MISSION; DESIGN; MODEL AB The dominant non-instrumental background source for space-based infrared observatories is the zodiacal light (ZL). We present Spitzer Infrared Array Camera (IRAC) measurements of the ZL at 3.6, 4.5, 5.8, and 8.0 mu m, taken as part of the instrument calibrations. We measure the changing surface brightness levels in approximately weekly IRAC observations near the north ecliptic pole over a period of roughly 8.5 years. This long time baseline is crucial for measuring the annual sinusoidal variation in the signal levels due to the tilt of the dust disk with respect to the ecliptic, which is the true signal of the ZL. This is compared to both Cosmic Background Explorer Diffuse Infrared Background Experiment data and a ZL model based thereon. Our data show a few-percent discrepancy from the Kelsall et al. model including a potential warping of the interplanetary dust disk and a previously detected overdensity in the dust cloud directly behind the Earth in its orbit. Accurate knowledge of the ZL is important for both extragalactic and Galactic astronomy including measurements of the cosmic infrared background, absolute measures of extended sources, and comparison to extrasolar interplanetary dust models. IRAC data can be used to further inform and test future ZL models. C1 [Krick, Jessica E.; Glaccum, William J.; Carey, Sean J.; Lowrance, Patrick J.; Surace, Jason A.; Ingalls, James G.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reach, William T.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Krick, JE (reprint author), CALTECH, Jet Prop Lab, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM jkrick@caltech.edu OI Hora, Joseph/0000-0002-5599-4650; Reach, William/0000-0001-8362-4094 FU National Aeronautics and Space Administration; National Science Foundation FX We thank the anonymous referee for useful suggestions on the manuscript. This research has made use of data from the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work was based on observations obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. 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. NR 16 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 JUL 20 PY 2012 VL 754 IS 1 AR 53 DI 10.1088/0004-637X/754/1/53 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800053 ER PT J AU Matheson, T Joyce, RR Allen, LE Saha, A Silva, DR Wood-Vasey, WM Adams, JJ Anderson, RE Beck, TL Bentz, MC Bershady, MA Binkert, WS Butler, K Camarata, MA Eigenbrot, A Everett, M Gallagher, JS Garnavich, PM Glikman, E Harbeck, D Hargis, JR Herbst, H Horch, EP Howell, SB Jha, S Kaczmarek, JF Knezek, P Manne-Nicholas, E Mathieu, RD Meixner, M Milliman, K Power, J Rajagopal, J Reetz, K Rhode, KL Schechtman-Rook, A Schwamb, ME Schweiker, H Simmons, B Simon, JD Summers, D Young, MD Weyant, A Wilcots, EM Will, G Williams, D AF Matheson, T. Joyce, R. R. Allen, L. E. Saha, A. Silva, D. R. Wood-Vasey, W. M. Adams, J. J. Anderson, R. E. Beck, T. L. Bentz, M. C. Bershady, M. A. Binkert, W. S. Butler, K. Camarata, M. A. Eigenbrot, A. Everett, M. Gallagher, J. S. Garnavich, P. M. Glikman, E. Harbeck, D. Hargis, J. R. Herbst, H. Horch, E. P. Howell, S. B. Jha, S. Kaczmarek, J. F. Knezek, P. Manne-Nicholas, E. Mathieu, R. D. Meixner, M. Milliman, K. Power, J. Rajagopal, J. Reetz, K. Rhode, K. L. Schechtman-Rook, A. Schwamb, M. E. Schweiker, H. Simmons, B. Simon, J. D. Summers, D. Young, M. D. Weyant, A. Wilcots, E. M. Will, G. Williams, D. TI THE INFRARED LIGHT CURVE OF SN 2011fe IN M101 AND THE DISTANCE TO M101 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; galaxies: individual (M101); supernovae: individual (SN 2011fe) ID HUBBLE-SPACE-TELESCOPE; SUPERNOVA LEGACY SURVEY; IA SUPERNOVAE; CEPHEID DISTANCES; DARK ENERGY; KEY PROJECT; ZERO-POINT; CONSTANT; PHOTOMETRY; CAMERA AB We present near-infrared light curves of supernova (SN) 2011fe in M101, including 34 epochs in H band starting 14 days before maximum brightness in the B band. The light curve data were obtained with the WIYN High-Resolution Infrared Camera. When the data are calibrated using templates of other Type Ia SNe, we derive an apparent H-band magnitude at the epoch of B-band maximum of 10.85 +/- 0.04. This implies a distance modulus for M101 that ranges from 28.86 to 29.17 mag, depending on which absolute calibration for Type Ia SNe is used. C1 [Matheson, T.; Joyce, R. R.; Allen, L. E.; Saha, A.; Silva, D. R.; Binkert, W. S.; Butler, K.; Everett, M.; Knezek, P.; Power, J.; Rajagopal, J.; Reetz, K.; Summers, D.; Will, G.; Williams, D.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Wood-Vasey, W. M.; Weyant, A.] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA. [Adams, J. J.; Simon, J. D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Anderson, R. E.; Beck, T. L.; Meixner, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bentz, M. C.; Manne-Nicholas, E.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Bershady, M. A.; Eigenbrot, A.; Gallagher, J. S.; Herbst, H.; Kaczmarek, J. F.; Mathieu, R. D.; Milliman, K.; Schechtman-Rook, A.; Wilcots, E. M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Bershady, M. A.; Horch, E. P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Garnavich, P. M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Glikman, E.; Schwamb, M. E.; Simmons, B.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Harbeck, D.; Knezek, P.; Schweiker, H.] WIYN Observ, Tucson, AZ 85719 USA. [Hargis, J. R.; Rhode, K. L.; Young, M. D.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Howell, S. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jha, S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Matheson, T (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. EM matheson@noao.edu OI Schwamb, Megan/0000-0003-4365-1455; Simmons, Brooke/0000-0001-5882-3323 FU WIYN Observatory FX We thank the referee, Mark Phillips, for extremely useful comments and suggestions. We also thank the WIYN Observatory for their support of this program. T. M. acknowledges many useful conversations with Chris Burns on the nature of SN light curves in the infrared. T. M. dedicates this paper to the memory of his friend and colleague, Dr. Weidong Li. NR 51 TC 30 Z9 30 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 JUL 20 PY 2012 VL 754 IS 1 AR 19 DI 10.1088/0004-637X/754/1/19 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800019 ER PT J AU Pancoast, A Brewer, BJ Treu, T Barth, AJ Bennert, VN Canalizo, G Filippenko, AV Gates, EL Greene, JE Li, WD Malkan, MA Sand, DJ Stern, D Woo, JH Assef, RJ Bae, HJ Buehler, T Cenko, SB Clubb, KI Cooper, MC Diamond-Stanic, AM Hiner, KD Honig, SF Joner, MD Kandrashoff, MT Laney, CD Lazarova, MS Nierenberg, AM Park, D Silverman, JM Son, D Sonnenfeld, A Thorman, SJ Tollerud, EJ Walsh, JL Walters, R AF Pancoast, Anna Brewer, Brendon J. Treu, Tommaso Barth, Aaron J. Bennert, Vardha N. Canalizo, Gabriela Filippenko, Alexei V. Gates, Elinor L. Greene, Jenny E. Li, Weidong Malkan, Matthew A. Sand, David J. Stern, Daniel Woo, Jong-Hak Assef, Roberto J. Bae, Hyun-Jin Buehler, Tabitha Cenko, S. Bradley Clubb, Kelsey I. Cooper, Michael C. Diamond-Stanic, Aleksandar M. Hiner, Kyle D. Hoenig, Sebastian F. Joner, Michael D. Kandrashoff, Michael T. Laney, C. David Lazarova, Mariana S. Nierenberg, A. M. Park, Dawoo Silverman, Jeffrey M. Son, Donghoon Sonnenfeld, Alessandro Thorman, Shawn J. Tollerud, Erik J. Walsh, Jonelle L. Walters, Richard TI THE LICK AGN MONITORING PROJECT 2011: DYNAMICAL MODELING OF THE BROAD-LINE REGION IN Mrk 50 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Mrk 50); galaxies: nuclei ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; REVERBERATION MAPPING DATA; SEYFERT-GALAXIES; BULGE RELATIONS; STRIPE 82; ARP 151; QUASARS; VARIABILITY; CALIBRATION AB We present dynamical modeling of the broad- line region (BLR) in the Seyfert 1 galaxy Mrk 50 using reverberation mapping data taken as part of the Lick AGN Monitoring Project (LAMP) 2011. We model the reverberation mapping data directly, constraining the geometry and kinematics of the BLR, as well as deriving a black hole mass estimate that does not depend on a normalizing factor or virial coefficient. We find that the geometry of the BLR in Mrk 50 is a nearly face-on thick disk, with a mean radius of 9.6(-0.9)(+1.2) light days, a width of the BLR of 6.9(-1.1)(+1.2) light days, and a disk opening angle of 25 +/- 10 deg above the plane. We also constrain the inclination angle to be 9(-5)(+7) deg, close to face-on. Finally, the black hole mass of Mrk 50 is inferred to be log(10)(M-BH/M-circle dot) = 7.57(-0.27)(+0.44). By comparison to the virial black hole mass estimate from traditional reverberation mapping analysis, we find the normalizing constant (virial coefficient) to be log(10) f = 0.78(-0.27)(+0.44), consistent with the commonly adopted mean value of 0.74 based on aligning the M-BH-sigma* relation for active galactic nuclei and quiescent galaxies. While our dynamical model includes the possibility of a net inflow or outflow in the BLR, we cannot distinguish between these two scenarios. C1 [Pancoast, Anna; Brewer, Brendon J.; Treu, Tommaso; Bennert, Vardha N.; Sand, David J.; Hoenig, Sebastian F.; Nierenberg, A. M.; Sonnenfeld, Alessandro] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Barth, Aaron J.; Cooper, Michael C.; Thorman, Shawn J.; Tollerud, Erik J.; Walsh, Jonelle L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bennert, Vardha N.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA. [Canalizo, Gabriela; Hiner, Kyle D.; Lazarova, Mariana S.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Filippenko, Alexei V.; Li, Weidong; Cenko, S. Bradley; Clubb, Kelsey I.; Kandrashoff, Michael T.; Silverman, Jeffrey M.] 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.] Las Cumbres Observ, Global Telescope Network, Santa Barbara, CA 93117 USA. [Stern, Daniel; Assef, Roberto J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Woo, Jong-Hak; Park, Dawoo; Son, Donghoon] 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; Joner, Michael D.; Laney, C. David] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. [Diamond-Stanic, Aleksandar M.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Silverman, Jeffrey M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Walsh, Jonelle L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Walters, Richard] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. RP Pancoast, A (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM pancoast@physics.ucsb.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-1107812, 1107865, 1108665, 1108835, AST-0618209, AST-0908886]; NSF; Packard Foundation; Southern California Center for Galaxy Evolution; University of California Office of Research; Richard & Rhoda Goldman Fund; NASA/Swift [NNX10AI21G, GO-7100028]; TABASGO Foundation; Deutsche Forschungsgemeinschaft (DFG); NASA; National Research Foundation of Korea; Ministry of Education, Science and Technology [2010-0021558] FX We thank the Lick Observatory staff for their exceptional support during our observing campaign. In addition, we thank Brandon Kelly for suggesting changes to our code that yielded significant improvements. The referee also provided valuable feedback that enabled us to improve the paper. The Lick AGN Monitoring Project 2011 is supported by NSF grants AST-1107812, 1107865, 1108665, and 1108835. The West Mountain Observatory is supported by NSF grant AST-0618209. A.P. acknowledges support from the NSF through the Graduate Research Fellowship Program. B.J.B. and T.T. acknowledge support from the Packard Foundation through a Packard Fellowship to T.T. A.D. acknowledges support from the Southern California Center for Galaxy Evolution, a multi-campus research program funded by the University of California Office of Research. A.V.F. and his group at UC Berkeley acknowledge generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. S.H. acknowledges support by Deutsche Forschungsgemeinschaft (DFG) in the framework of a research fellowship ("Auslandsstipendium"). The work of D.S. and R.A. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. J.H.W. acknowledges support by Basic Science Research Program through the National Research Foundation of Korea funded by the Ministry of Education, Science and Technology (2010-0021558). NR 38 TC 42 Z9 42 U1 0 U2 9 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 JUL 20 PY 2012 VL 754 IS 1 AR 49 DI 10.1088/0004-637X/754/1/49 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800049 ER PT J AU Rea, N Israel, GL Esposito, P Pons, JA Camero-Arranz, A Mignani, RP Turolla, R Zane, S Burgay, M Possenti, A Campana, S Enoto, T Gehrels, N Gogus, E Gotz, D Kouveliotou, C Makishima, K Mereghetti, S Oates, SR Palmer, DM Perna, R Stella, L Tiengo, A AF Rea, N. Israel, G. L. Esposito, P. Pons, J. A. Camero-Arranz, A. Mignani, R. P. Turolla, R. Zane, S. Burgay, M. Possenti, A. Campana, S. Enoto, T. Gehrels, N. Gogus, E. Goetz, D. Kouveliotou, C. Makishima, K. Mereghetti, S. Oates, S. R. Palmer, D. M. Perna, R. Stella, L. Tiengo, A. TI A NEW LOW MAGNETIC FIELD MAGNETAR: THE 2011 OUTBURST OF SWIFT J1822.3-1606 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (Swift J1822.3-1606); stars: magnetars; stars: neutron; X-rays: bursts; X-rays: stars ID X-RAY PULSAR; SOFT GAMMA REPEATER; NEUTRON-STARS; XTE J1810-197; SGR 0418+5729; SPIN-DOWN; EMISSION; SPECTRA; CATALOG; MODEL AB We report on the long-term X-ray monitoring with Swift, RXTE, Suzaku, Chandra, and XMM-Newton of the outburst of the newly discovered magnetar Swift J1822.3-1606 (SGR 1822-1606), from the first observations soon after the detection of the short X-ray bursts which led to its discovery, through the first stages of its outburst decay (covering the time span from 2011 July until the end of 2012 April). We also report on archival ROSAT observations which detected the source during its likely quiescent state, and on upper limits on Swift J1822.3-1606's radio-pulsed and optical emission during outburst, with the Green Bank Telescope and the Gran Telescopio Canarias, respectively. Our X-ray timing analysis finds the source rotating with a period of P = 8.43772016(2)s and a period derivative (P) over dot = 8.3(2) x10(-14) s s(-1), which implies an inferred dipolar surface magnetic field of B similar or equal to 2.7x10(13) G at the equator. This measurement makes Swift J1822.3-1606 the second lowest magnetic field magnetar (after SGR 0418+5729). Following the flux and spectral evolution from the beginning of the outburst, we find that the flux decreased by about an order of magnitude, with a subtle softening of the spectrum, both typical of the outburst decay of magnetars. By modeling the secular thermal evolution of Swift J1822.3-1606, we find that the observed timing properties of the source, as well as its quiescent X-ray luminosity, can be reproduced if it was born with a poloidal and crustal toroidal fields of B-p similar to 1.5x10(14) G and B-tor similar to 7x10(14) G, respectively, and if its current age is similar to 550 kyr. C1 [Rea, N.; Camero-Arranz, A.] Fac Ciencies, CSIC, Inst Ciencies Espai, IEEC, E-08193 Barcelona, Spain. [Israel, G. L.; Stella, L.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Esposito, P.; Burgay, M.; Possenti, A.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy. [Pons, J. A.] Univ Alacant, Dept Fis Aplicada, Alacant 03080, Spain. [Mignani, R. P.; Turolla, R.; Zane, S.; Oates, S. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Mignani, R. P.] Univ Zielona Gora, Inst Astron, PL-65265 Zielona Gora, Poland. [Turolla, R.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy. [Campana, S.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Enoto, T.] Stanford Univ, SLAC, KIPAC, Stanford, CA 94309 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gogus, E.] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. [Goetz, D.] Univ Paris Diderot, CNRS, CEA DSM, Irfu Serv Astrophys,AIM, F-91191 Gif Sur Yvette, France. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Makishima, K.] RIKEN, Inst Phys & Chem Res, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan. [Makishima, K.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Mereghetti, S.; Tiengo, A.] IASF Milano, INAF, I-20133 Milan, Italy. [Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Perna, R.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Tiengo, A.] IUSS Ist Univ Studi Super, I-27100 Pavia, Italy. RP Rea, N (reprint author), Fac Ciencies, CSIC, Inst Ciencies Espai, IEEC, Campus UAB,Torre C5 Parell, E-08193 Barcelona, Spain. RI PONS, JOSE/D-4687-2012; Lujan Center, LANL/G-4896-2012; Rea, Nanda/I-2853-2015; XRAY, SUZAKU/A-1808-2009; OI PONS, JOSE/0000-0003-1018-8126; Rea, Nanda/0000-0003-2177-6388; Israel, GianLuca/0000-0001-5480-6438; Campana, Sergio/0000-0001-6278-1576; Burgay, Marta/0000-0002-8265-4344; Tiengo, Andrea/0000-0002-6038-1090; MEREGHETTI, SANDRO/0000-0003-3259-7801; Esposito, Paolo/0000-0003-4849-5092 FU Ramon y Cajal Research Fellowship; Agenzia Spaziale Italiana (ASI); Ministero dell'Istruzione; Universita e Ricerca Scientifica e Tecnologica (MIUR-COFIN); Istituto Nazionale di Astrofisica (PRIN-INAF); Autonomous Region of Sardinia through the program PO Sardegna FSE "Promoting scientific research and innovation technology in Sardinia" [L.R. 7/2007]; NASA [NNH07ZDA001-GLAST]; [AYA2009-07391]; [SGR2009-811]; [TW2010005]; [iLINK 2011-0303] FX We are indebted to the Swift, RXTE, Chandra, Suzaku, and XMM-Newton scheduling teams for the extraordinary job in promptly planning all the observations presented in this paper. We acknowledge the extraordinary support of the GTC staff, and in particular Rene Rutten and Carlos Alvarez for the prompt reaction to our ToO trigger. We also thank the GBT staff for scheduling these ToO observations so efficiently. N.R. is supported by a Ramon y Cajal Research Fellowship, and by grants AYA2009-07391, SGR2009-811, TW2010005, and iLINK 2011-0303. The Italian authors are supported by Agenzia Spaziale Italiana (ASI), Ministero dell'Istruzione, Universita e Ricerca Scientifica e Tecnologica (MIUR-COFIN), and Istituto Nazionale di Astrofisica (PRIN-INAF) grants. P.E. acknowledges financial support from the Autonomous Region of Sardinia through a research grant under the program PO Sardegna FSE 2007-2013, L.R. 7/2007 "Promoting scientific research and innovation technology in Sardinia." C.K. was partially supported by NASA grant NNH07ZDA001-GLAST. NR 75 TC 71 Z9 72 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 JUL 20 PY 2012 VL 754 IS 1 AR 27 DI 10.1088/0004-637X/754/1/27 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800027 ER PT J AU Ricca, A Bauschlicher, CW Boersma, C Tielens, AGGM Allamandola, LJ AF Ricca, Alessandra Bauschlicher, Charles W., Jr. Boersma, Christiaan Tielens, Alexander G. G. M. Allamandola, Louis J. TI THE INFRARED SPECTROSCOPY OF COMPACT POLYCYCLIC AROMATIC HYDROCARBONS CONTAINING UP TO 384 CARBONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: general; methods: numerical; molecular data ID INTERSTELLAR-EMISSION FEATURE; BLIND SIGNAL SEPARATION; MU-M; FAR-IR; PAH MOLECULES; RED-RECTANGLE; SMALL GRAINS; ASTROPHYSICAL IMPLICATIONS; POLYAROMATIC HYDROCARBONS; REFLECTION NEBULAE AB The mid- and the far-infrared spectra of polycyclic aromatic hydrocarbons (PAHs) have been computed using density functional theory. This study has focused on PAHs in the highly symmetric, compact, coronene family with sizes up to 384 carbons. We have identified trends in the peak position and intrinsic strength of the vibrational modes of these species and compared these to trends previously reported for less symmetric and smaller PAHs. The computed spectral modes have been used to calculate the IR emission spectrum of PAHs pumped by UV photons. The results have been compared to observed interstellar spectra to elucidate the characteristics of the interstellar PAH family. The calculations show that highly symmetric PAHs are very stable and, hence, might be favored under the harsh conditions of interstellar space. Our calculated vibrational properties confirm and extend previous studies for small PAHs to the large compact PAHs studied here, specifically in terms of the dependence of the spectral characteristics on ionization and on H-adjacency. The calculations show that for PAHs larger than 150 carbons, the 6.3 mu m feature becomes very broad and shifts to longer wavelengths, the 8.6 mu m band becomes stronger than the "7.7" mu m band, and the 11.0/12.7 band strength ratio gets too large compared with observations. Thus, PAHs with 150 carbons or more are unlikely to be the dominant species in interstellar space. The simplicity of the observed spectra in the 15-20 mu m range points toward a preponderance of compact PAHs in the interstellar PAH family. C1 [Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Bauschlicher, Charles W., Jr.] NASA Ames Res Ctr, Entry Syst & Technol Div, Mail Stop 230 3, Moffett Field, CA 94035 USA. [Boersma, Christiaan; Allamandola, Louis J.] NASA Ames Res Ctr, Div Space Sci, Mail Stop 230 3, Moffett Field, CA 94035 USA. [Tielens, Alexander G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Ricca, A (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM Alessandra.Ricca-1@nasa.gov; Charles.W.Bauschlicher@nasa.gov; Christiaan.Boersma@nasa.gov; tielens@strw.leidenuniv.nl; Louis.J.Allamandola@nasa.gov RI Boersma, Christiaan/L-7696-2014 OI Boersma, Christiaan/0000-0002-4836-217X FU NASA Astrobiology and Laboratory Astrophysics programs; NASA; ERC from the European Research Council [246976]; Dutch Astrochemistry Network; Dutch Science Organization, NWO FX A.R. thanks NASA's Astrophysics Theory and Fundamental Physics (ATFP; NNX09AD18G) program for its generous support of this work. We also acknowledge support from NASA Astrobiology and Laboratory Astrophysics programs. This work was supported through an appointment (C.B.) to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. Studies of interstellar PAHs at Leiden Observatory are supported through advanced-ERC grant 246976 from the European Research Council and through the Dutch Astrochemistry Network funded by the Dutch Science Organization, NWO. NR 102 TC 44 Z9 44 U1 3 U2 55 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 JUL 20 PY 2012 VL 754 IS 1 AR 75 DI 10.1088/0004-637X/754/1/75 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800075 ER PT J AU Savage, SL Holman, G Reeves, KK Seaton, DB McKenzie, DE Su, Y AF Savage, Sabrina L. Holman, Gordon Reeves, Katharine K. Seaton, Daniel B. McKenzie, David E. Su, Yang TI LOW-ALTITUDE RECONNECTION INFLOW-OUTFLOW OBSERVATIONS DURING A 2010 NOVEMBER 3 SOLAR ERUPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic topology; Sun: UV radiation; Sun: X-rays, gamma rays ID SUPRA-ARCADE DOWNFLOWS; MAGNETIC RECONNECTION; CURRENT SHEET; QUANTITATIVE EXAMINATION; PATCHY RECONNECTION; FLARE PLASMA; MODEL; EJECTION; EMISSIONS; MOTIONS AB For a solar flare occurring on 2010 November 3, we present observations using several SDO/AIA extreme-ultraviolet (EUV) passbands of an erupting flux rope followed by inflows sweeping into a current sheet region. The inflows are soon followed by outflows appearing to originate from near the termination point of the inflowing motion-an observation in line with standard magnetic reconnection models. We measure average inflow plane-of-sky speeds to range from similar to 150 to 690 km s(-1) with the initial, high-temperature inflows being the fastest. Using the inflow speeds and a range of Alfven speeds, we estimate the Alfvenic Mach number which appears to decrease with time. We also provide inflow and outflow times with respect to RHESSI count rates and find that the fast, high-temperature inflows occur simultaneously with a peak in the RHESSI thermal light curve. Five candidate inflow-outflow pairs are identified with no more than a minute delay between detections. The inflow speeds of these pairs are measured to be similar to 10(2) km s(-1) with outflow speeds ranging from similar to 10(2) to 10(3) km s(-1)-indicating acceleration during the reconnection process. The fastest of these outflows are in the form of apparently traveling density enhancements along the legs of the loops rather than the loop apexes themselves. These flows could possibly either be accelerated plasma, shocks, or waves prompted by reconnection. The measurements presented here show an order of magnitude difference between the retraction speeds of the loops and the speed of the density enhancements within the loops-presumably exiting the reconnection site. C1 [Savage, Sabrina L.; Holman, Gordon; Su, Yang] Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Seaton, Daniel B.] Royal Observ Belgium SIDC, B-1180 Brussels, Belgium. [McKenzie, David E.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Su, Yang] Graz Univ, Inst Phys, A-8010 Graz, Austria. RP Savage, SL (reprint author), Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 671, Greenbelt, MD 20771 USA. RI Su, Yang/J-5381-2014; Reeves, Katharine/P-9163-2014; OI SEATON, DANIEL/0000-0002-0494-2025 FU NASA HGI; RHESSI; Lockheed-Martin [SP02H1701R, SP02H3901R]; PRODEX [C90345]; PROBA2/SWAP mission; European Commission [218816] FX S. L. Savage is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center administered by Oak Ridge Associated Universities through a contract with NASA and under the mentorship of G. Holman. G. Holman is supported by a NASA HGI Grant and the RHESSI program. K. K. Reeves is supported under contract SP02H1701R from Lockheed-Martin to SAO. Support for D.B.S.'s contribution to this paper came from PRODEX Grant No. C90345 managed by the European Space Agency in collaboration with the Belgian Federal Science Policy Office (BELSPO) in support of the PROBA2/SWAP mission, and from the European Commission's Seventh Framework Programme (FP7/2007-2013) under the grant agreement no. 218816 (SOTERIA project, www.soteria-space.eu). D. E. McKenzie is supported under contract SP02H3901R from Lockheed-Martin to MSU. The authors thank Dr. Nicholas Murphy for valuable discussions and the anonymous referee for enhancing the manuscript. NR 56 TC 25 Z9 25 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 JUL 20 PY 2012 VL 754 IS 1 AR 13 DI 10.1088/0004-637X/754/1/13 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800013 ER PT J AU Tanvir, NR Levan, AJ Fruchter, AS Fynbo, JPU Hjorth, J Wiersema, K Bremer, MN Rhoads, J Jakobsson, P O'Brien, PT Stanway, ER Bersier, D Natarajan, P Greiner, J Watson, D Castro-Tirado, AJ Wijers, RAMJ Starling, RLC Misra, K Graham, JF Kouveliotou, C AF Tanvir, N. R. Levan, A. J. Fruchter, A. S. Fynbo, J. P. U. Hjorth, J. Wiersema, K. Bremer, M. N. Rhoads, J. Jakobsson, P. O'Brien, P. T. Stanway, E. R. Bersier, D. Natarajan, P. Greiner, J. Watson, D. Castro-Tirado, A. J. Wijers, R. A. M. J. Starling, R. L. C. Misra, K. Graham, J. F. Kouveliotou, C. TI STAR FORMATION IN THE EARLY UNIVERSE: BEYOND THE TIP OF THE ICEBERG SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: luminosity function, mass function ID GAMMA-RAY-BURST; ULTRA-DEEP-FIELD; HUBBLE-SPACE-TELESCOPE; LYMAN-BREAK GALAXIES; SIMILAR-TO 7; CORE-COLLAPSE SUPERNOVAE; HIGH COLUMN DENSITY; HOST GALAXY; HIGH-REDSHIFT; WFC3/IR OBSERVATIONS AB We present late-time Hubble Space Telescope (HST) imaging of the fields of six Swift gamma-ray bursts (GRBs) lying at 5.0 less than or similar to z less than or similar to 9.5. Our data include very deep observations of the field of the most distant spectroscopically confirmed burst, GRB 090423, at z = 8.2. Using the precise positions afforded by their afterglows, we can place stringent limits on the luminosities of their host galaxies. In one case, that of GRB 060522 at z = 5.11, there is a marginal excess of flux close to the GRB position which may be a detection of a host at a magnitude J(AB) approximate to 28.5. None of the others are significantly detected, meaning that all the hosts lie below L* at their respective redshifts, with star formation rates (SFRs) less than or similar to 4 M-circle dot yr(-1) in all cases. Indeed, stacking the five fields with WFC3-IR data, we conclude a mean SFR < 0.17 M-circle dot yr(-1) per galaxy. These results support the proposition that the bulk of star formation, and hence integrated UV luminosity, at high redshifts arises in galaxies below the detection limits of deep-field observations. Making the reasonable assumption that GRB rate is proportional to UV luminosity at early times allows us to compare our limits with expectations based on galaxy luminosity functions (LFs) derived from the Hubble Ultra-Deep Field and other deep fields. We infer that an LF, which is evolving rapidly toward steeper faint-end slope (alpha) and decreasing characteristic luminosity (L*), as suggested by some other studies, is consistent with our observations, whereas a non-evolving LF shape is ruled out at greater than or similar to 90% confidence. Although it is not yet possible to make stronger statements, in the future, with larger samples and a fuller understanding of the conditions required for GRB production, studies like this hold great potential for probing the nature of star formation, the shape of the galaxy LF, and the supply of ionizing photons in the early universe. C1 [Tanvir, N. R.; Wiersema, K.; O'Brien, P. T.; Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Levan, A. J.; Stanway, E. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Fruchter, A. S.; Misra, K.; Graham, J. F.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fynbo, J. P. U.; Hjorth, J.; Watson, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Bremer, M. N.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Rhoads, J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England. [Natarajan, P.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Natarajan, P.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA USA. [Greiner, J.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Castro-Tirado, A. J.] Inst Astrofs Andalucia IAA CSIC, Granada 18008, Spain. [Wijers, R. A. M. J.] Astron Inst Anton Pannekoek, NL-1090 SJ Amsterdam, Netherlands. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Tanvir, NR (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM nrt3@star.le.ac.uk RI Fynbo, Johan/L-8496-2014; Watson, Darach/E-4521-2015; Jakobsson, Pall/L-9950-2015; OI Fynbo, Johan/0000-0002-8149-8298; Watson, Darach/0000-0002-4465-8264; Jakobsson, Pall/0000-0002-9404-5650; Stanway, Elizabeth/0000-0002-8770-809X; Wijers, Ralph/0000-0002-3101-1808; Castro-Tirado, A. J./0000-0003-2999-3563 FU STFC; NASA [NAS 5-26555]; ERC-StG [EGGS-278202]; DNRF FX We acknowledge support from STFC. Based on observations made with the NASA/ESA Hubble Space Telescope (HST), obtained from the data archive at the Space Telescope Institute. STScI is operated by the association of Universities for Research in Astronomy, Inc. under the NASA contract NAS 5-26555. These observations are associated with HST programs GO-10616 (PI: Berger), GO-10926 (PI: Tanvir), GO-11189 (PI: Tanvir), and GO-11734 (PI: Levan).; J.P.U.F. acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. NR 99 TC 64 Z9 64 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2012 VL 754 IS 1 AR 46 DI 10.1088/0004-637X/754/1/46 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800046 ER PT J AU Tassis, K Willacy, K Yorke, HW Turner, NJ AF Tassis, Konstantinos Willacy, Karen Yorke, Harold W. Turner, Neal J. TI NON-EQUILIBRIUM CHEMISTRY OF DYNAMICALLY EVOLVING PRESTELLAR CORES. II. IONIZATION AND MAGNETIC FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: clouds; ISM: molecules; magnetic fields; magnetohydrodynamics (MHD); stars: formation ID MASS STAR-FORMATION; CLOUD CORES; AMBIPOLAR-DIFFUSION; MOLECULAR CLOUDS; DENSE CORES; DARK CLOUDS; AXISYMMETRICAL SOLUTIONS; INTERSTELLAR CLOUDS; PROTOSTAR FORMATION; ZEEMAN OBSERVATIONS AB We study the effect that non-equilibrium chemistry in dynamical models of collapsing molecular cloud cores has on measurements of the magnetic field in these cores, the degree of ionization, and the mean molecular weight of ions. We find that OH and CN, usually used in Zeeman observations of the line-of-sight magnetic field, have an abundance that decreases toward the center of the core much faster than the density increases. As a result, Zeeman observations tend to sample the outer layers of the core and consistently underestimate the core magnetic field. The degree of ionization follows a complicated dependence on the number density at central densities up to 10(5) cm(-3) for magnetic models and 10(6) cm(-3) in non-magnetic models. At higher central densities, the scaling approaches a power law with a slope of -0.6 and a normalization which depends on the cosmic-ray ionization rate zeta and the temperature T as (zeta T)(1/2). The mean molecular weight of ions is systematically lower than the usually assumed value of 20-30, and, at high densities, approaches a value of 3 due to the asymptotic dominance of the H-3(+) ion. This significantly lower value implies that ambipolar diffusion operates faster. C1 [Tassis, Konstantinos; Willacy, Karen; Yorke, Harold W.; Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tassis, K (reprint author), Max Planck Inst Radioastron, D-53121 Bonn, Germany. RI Tassis, Konstantinos/C-3155-2011; OI Tassis, Konstantinos/0000-0002-8831-2038; Turner, Neal/0000-0001-8292-1943 NR 40 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2012 VL 754 IS 1 AR 6 DI 10.1088/0004-637X/754/1/6 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800006 ER PT J AU Usmanov, AV Goldstein, ML Matthaeus, WH AF Usmanov, Arcadi V. Goldstein, Melvyn L. Matthaeus, William H. TI THREE-DIMENSIONAL MAGNETOHYDRODYNAMIC MODELING OF THE SOLAR WIND INCLUDING PICKUP PROTONS AND TURBULENCE TRANSPORT SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; magnetohydrodynamics (MHD); methods: numerical; solar wind; turbulence ID LOCAL INTERSTELLAR-MEDIUM; PRESSURE-BALANCED STRUCTURES; ELECTRON HEAT-CONDUCTION; OUTER HELIOSPHERE; TERMINATION SHOCK; MAGNETIC-FIELD; DISTANT HELIOSPHERE; COROTATING STREAMS; NEUTRAL HYDROGEN; MHD SIMULATION AB To study the effects of interstellar pickup protons and turbulence on the structure and dynamics of the solar wind, we have developed a fully three-dimensional magnetohydrodynamic solar wind model that treats interstellar pickup protons as a separate fluid and incorporates the transport of turbulence and turbulent heating. The governing system of equations combines the mean-field equations for the solar wind plasma, magnetic field, and pickup protons and the turbulence transport equations for the turbulent energy, normalized cross-helicity, and correlation length. The model equations account for photoionization of interstellar hydrogen atoms and their charge exchange with solar wind protons, energy transfer from pickup protons to solar wind protons, and plasma heating by turbulent dissipation. Separate mass and energy equations are used for the solar wind and pickup protons, though a single momentum equation is employed under the assumption that the pickup protons are comoving with the solar wind protons. We compute the global structure of the solar wind plasma, magnetic field, and turbulence in the region from 0.3 to 100 AU for a source magnetic dipole on the Sun tilted by 0 degrees-90 degrees and compare our results with Voyager 2 observations. The results computed with and without pickup protons are superposed to evaluate quantitatively the deceleration and heating effects of pickup protons, the overall compression of the magnetic field in the outer heliosphere caused by deceleration, and the weakening of corotating interaction regions by the thermal pressure of pickup protons. C1 [Usmanov, Arcadi V.; Matthaeus, William H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Usmanov, Arcadi V.; Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Usmanov, AV (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. EM arcadi.usmanov@nasa.gov RI Usmanov, Arcadi/A-9860-2013 FU NSF/DOE [AST-1004035]; NASA [NNX09AH79G, NNX08AI47G]; NSF [AGS-1063439, SHINE ATM-0752135] FX We acknowledge the use of Voyager 2 data supplied by the National Space Science Data Center. The work of A.V.U. was supported by the NSF/DOE Partnership in Basic Plasma Science and Engineering Program grant AST-1004035, and by NASA grant NNX09AH79G to the University of Delaware. W.H.M. was partially supported by the NASA Heliophysics Theory Program NNX08AI47G and by the NSF Solar Terrestrial Program AGS-1063439 and SHINE ATM-0752135. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at the Ames Research Center and the NASA Center for Climate Simulation (NCCS) at the Goddard Space Flight Center. NR 99 TC 15 Z9 15 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 JUL 20 PY 2012 VL 754 IS 1 AR 40 DI 10.1088/0004-637X/754/1/40 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800040 ER PT J AU Yizengaw, E Zesta, E Moldwin, MB Damtie, B Mebrahtu, A Valladares, CE Pfaff, RF AF Yizengaw, E. Zesta, E. Moldwin, M. B. Damtie, B. Mebrahtu, A. Valladares, C. E. Pfaff, R. F. TI Longitudinal differences of ionospheric vertical density distribution and equatorial electrodynamics SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID TOTAL ELECTRON-CONTENT; TOMOGRAPHY; STORM; LATITUDES; SPACE AB Accurate estimation of global vertical distribution of ionospheric and plasmaspheric density as a function of local time, season, and magnetic activity is required to improve the operation of space-based navigation and communication systems. The vertical density distribution, especially at low and equatorial latitudes, is governed by the equatorial electrodynamics that produces a vertical driving force. The vertical structure of the equatorial density distribution can be observed by using tomographic reconstruction techniques on ground-based global positioning system (GPS) total electron content (TEC). Similarly, the vertical drift, which is one of the driving mechanisms that govern equatorial electrodynamics and strongly affect the structure and dynamics of the ionosphere in the low/midlatitude region, can be estimated using ground magnetometer observations. We present tomographically reconstructed density distribution and the corresponding vertical drifts at two different longitudes: the East African and west South American sectors. Chains of GPS stations in the east African and west South American longitudinal sectors, covering the equatorial anomaly region of meridian similar to 37 degrees E and 290 degrees E, respectively, are used to reconstruct the vertical density distribution. Similarly, magnetometer sites of African Meridian B-field Education and Research (AMBER) and INTERMAGNET for the east African sector and South American Meridional B-field Array (SAMBA) and Low Latitude Ionospheric Sensor Network (LISN) are used to estimate the vertical drift velocity at two distinct longitudes. The comparison between the reconstructed and Jicamarca Incoherent Scatter Radar (ISR) measured density profiles shows excellent agreement, demonstrating the usefulness of tomographic reconstruction technique in providing the vertical density distribution at different longitudes. Similarly, the comparison between magnetometer estimated vertical drift and other independent drift observation, such as from VEFI onboard Communication/Navigation Outage Forecasting System (C/NOFS) satellite and JULIA radar, is equally promising. The observations at different longitudes suggest that the vertical drift velocities and the vertical density distribution have significant longitudinal differences; especially the equatorial anomaly peaks expand to higher latitudes more in American sector than the African sector, indicating that the vertical drift in the American sector is stronger than the African sector. C1 [Yizengaw, E.; Valladares, C. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Zesta, E.] USA, Res Lab, AFRL VSBXP, Hanscom AFB, Bedford, MA USA. [Moldwin, M. B.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Damtie, B.] Bahir Dar Univ, Washera Geospace & Radar Sci Lab, Bahir Dar, Ethiopia. [Mebrahtu, A.] Mekelle Univ, Dept Phys, Mekelle, Ethiopia. [Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yizengaw, E (reprint author), Boston Coll, Inst Sci Res, 140 Commonwealth Ave, Chestnut Hill, MA 02467 USA. EM endawoke.kassie@bc.edu RI Pfaff, Robert/F-5703-2012; Moldwin, Mark/F-8785-2011; Yizengaw, Endawoke/I-3471-2015 OI Pfaff, Robert/0000-0002-4881-9715; Moldwin, Mark/0000-0003-0954-1770; Yizengaw, Endawoke/0000-0001-5772-3355 FU NASA IHY program [NNX07AM22G]; NASA LWS program [NNX11AP02G, NNX10AQ53G]; NASA Geospace Science program [NNX09AR84G]; AFOSR YIP grant [FA9550-10-1-0096] FX This work was supported by NASA IHY (NNX07AM22G), LWS (NNX11AP02G and NNX10AQ53G) and Geospace Science programs (NNX09AR84G) and AFOSR YIP grant (FA9550-10-1-0096). The authors are indebted to the IGS and UNAVCO GPS, Jicamarca radar, and INTERMAGNET magnetometer teams for the data resources they made available to the public. NR 30 TC 10 Z9 10 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 JUL 19 PY 2012 VL 117 AR A07312 DI 10.1029/2011JA017454 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977YN UT WOS:000306701700002 ER PT J AU Gao, F Anderson, MC Kustas, WP Wang, YJ AF Gao, Feng Anderson, Martha C. Kustas, William P. Wang, Yujie TI Simple method for retrieving leaf area index from Landsat using MODIS leaf area index products as reference SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE leaf area index; Landsat; MODIS; SMEX02 field campaign ID SURFACE REFLECTANCE; VEGETATION; ALGORITHM; FLUXES; HETEROGENEITY; VALIDATION; FRACTION; IMAGERY; ENERGY; MODEL AB Leaf area index (LAI) is a key parameter in most land surface models. Models that operate at multiple spatial scales may require consistent LAI inputs at different spatial resolutions or from different sensors. For example, the atmosphere-land exchange inverse model and associated disaggregation algorithm (DisALEXI) use the moderate resolution imaging spectro-radiometer (MODIS) LAI product to model fluxes at regional scales (1- to 10-km grid resolution), and Landsat-based LAI to disaggregate to field scale (30-m grid). In order to make a MODIS-consistent LAI product from Landsat imagery for this combined scheme, a simple reference-based regression tree approach was developed. This approach uses homogeneous and high-quality LAI retrievals from MODIS as references to develop a regression tree relating these MODIS LAI samples to Landsat surface reflectances. Results show that the approach can produce accurate estimates of LAI from Landsat, as evaluated using field measurements collected during the soil moisture experiment of 2002, conducted in central Iowa during a period of rapid vegetation growth. The coefficient of determination (r(2)) computed between Landsat retrievals and field measurements was 0.94 at the field scale, with an overall mean bias error (MBE) of -0.07 and mean absolute difference (MAD) of 0.23. MAD values of 0.17 and 0.32 were obtained for low to moderate LAI (0-3) and high LAI (>3), respectively, with some underestimation for the high LAI (MBE -0.28). The LAI maps retrieved from Landsat were consistent with the MODIS estimates when aggregated to coarser scales. MAD computed between Landsat- and MODIS-derived LAI ranged from 0.07 to 0.83 for different Landsat dates, with no significant bias compared to MODIS high-quality retrievals. This approach demonstrates a simple framework for producing MODIS-consistent LAI from Landsat data for modeling the land surface at different spatial scales. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.JRS.6.063554] C1 [Gao, Feng; Anderson, Martha C.; Kustas, William P.] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Wang, Yujie] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Gao, F (reprint author), ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. EM Feng.Gao@ars.usda.gov RI Anderson, Martha/C-1720-2015; Kustas, William/C-2063-2015 OI Anderson, Martha/0000-0003-0748-5525; FU U.S. Geological Survey (USGS) Landsat Data Continuity Mission (LDCM) Science Team program; NASA Earth Observing System (EOS) program FX This work was supported by the U.S. Geological Survey (USGS) Landsat Data Continuity Mission (LDCM) Science Team program and the NASA Earth Observing System (EOS) program. Special thanks go to A. Stern and B. Akhmedou for providing additional LAI field measurements in Walnut Creek watershed published by Dr. P. C. Doraiswamy, and to Dr. P. Beeson for valuable discussions. The U. S. Department of Agriculture (USDA) prohibits discrimination in all its programs and activities on the basis of race, color, national origin, age, disability, and where applicable, sex, marital status, familial status, parental status, religion, sexual orientation, genetic information, political beliefs, reprisal, or because all or part of an individual's income is derived from any public assistance program. (Not all prohibited bases apply to all programs.) Persons with disabilities who require alternative means for communication of program information (Braille, large print, audiotape, etc.) should contact USDA's TARGET Center at (202) 7202600 (voice and TDD). To file a complaint of discrimination, write to USDA, Director, Office of Civil Rights, 1400 Independence Avenue, S. W., Washington, D. C. 20250-9410, or call (800) 795-3272 (voice) or (202) 720-6382 (TDD). USDA is an equal opportunity provider and employer. NR 31 TC 19 Z9 20 U1 1 U2 31 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 JUL 18 PY 2012 VL 6 AR 063554 DI 10.1117/1.JRS.6.063554 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 994OX UT WOS:000307941600001 ER PT J AU Bahcivan, H Cutler, JW Bennett, M Kempke, B Springmann, JC Buonocore, J Nicolls, M Doe, R AF Bahcivan, H. Cutler, J. W. Bennett, M. Kempke, B. Springmann, J. C. Buonocore, J. Nicolls, M. Doe, R. TI First measurements of radar coherent scatter by the Radio Aurora Explorer CubeSat SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ELECTRON-DRIFT VELOCITY; UNSTABLE PLASMA-WAVES; POLAR E-REGION; EQUATORIAL ELECTROJET; STARE VELOCITIES; IRREGULARITIES; INSTABILITY; IONOSPHERE AB The Radio Aurora Explorer CubeSat detected the first radar echoes during the solar storm of March 8, 2012. The 300 s ground-to-space bi-static radar experiment was conducted in conjunction with the Poker Flat Incoherent Scatter Radar in the local morning (similar to 8 am) over Poker Flat, Alaska. The geomagnetic conditions for the E region field-aligned irregularity generation were optimal due to strong (about 1500 m/s) F region ion drifts and sufficient E region ionization (electron densities were similar to 2 x 10(11) m(-3)). The corresponding E region electric field of similar to 80 mV/m was larger than the excitation threshold for the Farley-Buneman instability. An auto-correlation analysis resolved, for the first time, the distribution of auroral E region backscatter with 3 km resolution in altitude and sub-degree resolution in aspect angle. Moreover, the measured Doppler velocities of the UHF scatter shows the phase speed saturation of the meter-scale plasma waves. The measured Doppler velocity is in excellent agreement with the C-s cos theta formula for auroral E region irregularities. Citation: Bahcivan, H., J. W. Cutler, M. Bennett, B. Kempke, J. C. Springmann, J. Buonocore, M. Nicolls, and R. Doe (2012), First measurements of radar coherent scatter by the Radio Aurora Explorer CubeSat, Geophys. Res. Lett., 39, L14101, doi: 10.1029/2012GL052249. C1 [Bahcivan, H.; Buonocore, J.; Nicolls, M.; Doe, R.] SRI Int, Ctr Geospace Studies, Menlo Pk, CA 94025 USA. [Cutler, J. W.; Kempke, B.; Springmann, J. C.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. [Bennett, M.] NASA, Jet Prop Lab, Pasadena, CA USA. RP Bahcivan, H (reprint author), SRI Int, Ctr Geospace Studies, 333 Ravenswood Ave,G284, Menlo Pk, CA 94025 USA. EM hasan.bahcivan@sri.com RI Nicolls, Michael/N-8680-2013 OI Nicolls, Michael/0000-0001-8267-6327 FU National Science Foundation [ATM-0121483]; NSF [ATM-0608577] FX RAX was developed under National Science Foundation grant ATM-0121483 to SRI International and the University of Michigan. PFISR operations and maintenance is supported by NSF cooperative agreement ATM-0608577 to SRI International. NR 18 TC 5 Z9 5 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 18 PY 2012 VL 39 AR L14101 DI 10.1029/2012GL052249 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 977YF UT WOS:000306700700001 ER PT J AU Jiang, JH Su, H Zhai, CX Perun, VS Del Genio, A Nazarenko, LS Donner, LJ Horowitz, L Seman, C Cole, J Gettelman, A Ringer, MA Rotstayn, L Jeffrey, S Wu, TW Brient, F Dufresne, JL Kawai, H Koshiro, T Watanabe, M LEcuyer, TS Volodin, EM Iversen, T Drange, H Mesquita, MDS Read, WG Waters, JW Tian, BJ Teixeira, J Stephens, GL AF Jiang, Jonathan H. Su, Hui Zhai, Chengxing Perun, Vincent S. Del Genio, Anthony Nazarenko, Larissa S. Donner, Leo J. Horowitz, Larry Seman, Charles Cole, Jason Gettelman, Andrew Ringer, Mark A. Rotstayn, Leon Jeffrey, Stephen Wu, Tongwen Brient, Florent Dufresne, Jean-Louis Kawai, Hideaki Koshiro, Tsuyoshi Watanabe, Masahiro LEcuyer, Tristan S. Volodin, Evgeny M. Iversen, Trond Drange, Helge Mesquita, Michel D. S. Read, William G. Waters, Joe W. Tian, Baijun Teixeira, Joao Stephens, Graeme L. TI Evaluation of cloud and water vapor simulations in CMIP5 climate models using NASA "A-Train" satellite observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODELS; TROPICAL DEEP CONVECTION; SEASONAL-VARIATION; VERTICAL STRUCTURE; AURA MLS; CAM-OSLO; GCM; SENSITIVITY; FEEDBACK; VARIABILITY AB Using NASA's A-Train satellite measurements, we evaluate the accuracy of cloud water content (CWC) and water vapor mixing ratio (H2O) outputs from 19 climate models submitted to the Phase 5 of Coupled Model Intercomparison Project (CMIP5), and assess improvements relative to their counterparts for the earlier CMIP3. We find more than half of the models show improvements from CMIP3 to CMIP5 in simulating column-integrated cloud amount, while changes in water vapor simulation are insignificant. For the 19 CMIP5 models, the model spreads and their differences from the observations are larger in the upper troposphere (UT) than in the lower or middle troposphere (L/MT). The modeled mean CWCs over tropical oceans range from similar to 3% to similar to 15 x of the observations in the UT and 40% to 2 x of the observations in the L/MT. For modeled H2Os, the mean values over tropical oceans range from similar to 1% to 2 x of the observations in the UT and within 10% of the observations in the L/MT. The spatial distributions of clouds at 215 hPa are relatively well-correlated with observations, noticeably better than those for the L/MT clouds. Although both water vapor and clouds are better simulated in the L/MT than in the UT, there is no apparent correlation between the model biases in clouds and water vapor. Numerical scores are used to compare different model performances in regards to spatial mean, variance and distribution of CWC and H2O over tropical oceans. Model performances at each pressure level are ranked according to the average of all the relevant scores for that level. C1 [Jiang, Jonathan H.; Su, Hui; Zhai, Chengxing; Perun, Vincent S.; Read, William G.; Waters, Joe W.; Tian, Baijun; Teixeira, Joao; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Del Genio, Anthony; Nazarenko, Larissa S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Donner, Leo J.; Horowitz, Larry; Seman, Charles] Geophys Fluid Dynam Lab, Princeton, NJ USA. [Cole, Jason] Environm Canada, Canadian Ctr Climate Modeling & Anal, Toronto, ON, Canada. [Gettelman, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Ringer, Mark A.] Met Off Hadley Ctr, Exeter, Devon, England. [Rotstayn, Leon] Commonwealth Sci & Ind Res Org, Clayton, Vic, Australia. [Jeffrey, Stephen] Queensland Climate Change Ctr Excellence, Dutton Pk, Qld, Australia. [Wu, Tongwen] China Meteorol Adm, Beijing Climate Ctr, Beijing, Peoples R China. [Brient, Florent; Dufresne, Jean-Louis] Inst Pierre Simon Laplace, Lab Meteorologie Dynam, Paris, France. [Kawai, Hideaki; Koshiro, Tsuyoshi] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan. [Watanabe, Masahiro] Univ Tokyo, Model Interdisciplinary Res Climate Atmospher & O, Chiba, Japan. [LEcuyer, Tristan S.] Univ Wisconsin, Madison, WI USA. [Volodin, Evgeny M.] Russian Acad Sci, Inst Numer Math, Moscow, Russia. [Iversen, Trond] Norwegian Climate Ctr, Meteorol Inst, Oslo, Norway. [Drange, Helge; Mesquita, Michel D. S.] Bjerknes Ctr Climate Res, Uni Res, Bergen, Norway. RP Jiang, JH (reprint author), CALTECH, Jet Prop Lab, MS 183-701,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jonathan.h.jiang@jpl.nasa.gov RI L'Ecuyer, Tristan/C-7040-2013; Rotstayn, Leon/A-1756-2012; Horowitz, Larry/D-8048-2014; L'Ecuyer, Tristan/E-5607-2012; Dufresne, Jean-Louis/I-5616-2015; Mesquita, Michel d. S./C-3414-2009; Koshiro, Tsuyoshi/O-7183-2016; Tian, Baijun/A-1141-2007; Ringer, Mark/E-7294-2013 OI Rotstayn, Leon/0000-0002-2385-4223; Horowitz, Larry/0000-0002-5886-3314; L'Ecuyer, Tristan/0000-0002-7584-4836; Dufresne, Jean-Louis/0000-0003-4764-9600; Mesquita, Michel d. S./0000-0002-4556-5414; Koshiro, Tsuyoshi/0000-0003-2971-7446; Cole, Jason/0000-0003-0450-2748; Tian, Baijun/0000-0001-9369-2373; Ringer, Mark/0000-0003-4014-2583 FU Aura MLS team; Climate Science Center at the Jet Propulsion Laboratory; California Institute of Technology; NASA; CloudSat project; NASA CloudSat Science [NAS5-99237]; Joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101] FX The NASA ROSES10 AST and COUND programs fund this project. The authors acknowledge the supports by the Aura MLS team and the Climate Science Center at the Jet Propulsion Laboratory, California Institute of Technology, sponsored by NASA. Jonathan Jiang and Hui Su are also grateful to Debbie Vane and CloudSat project for support; Tristan L'Ecuyer thanks the NASA CloudSat Science grant NAS5-99237; Mark Ringer acknowledges the support by the Joint DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). We thank helpful discussion and comments from Peter Gleckler, Karl Taylor, Stephen Klein and Curt Covey of PCMDI, Lawrence Livermore National Laboratory; Veronika Eyring of Institute of Atmospheric Physics, Germany; William Rossow of City College of New York; Mark Schoeberl of Science and Technology Corporation; Brian Kahn of the AIRS team; Stephen Platnick of the MODIS team; and Melody Avery of the CALIPSO team. The three internal reviewers from CCCMA and CSIRO, as well as the three anonymous reviewers of this journal, provided constructive comments. We are also very thankful to our colleagues from climate modeling centers across the globe, including BCC, BCCR, CCCMA, CNRM, QCCCE, CSIRO, GFDL, GISS, INM, IPSL, MIROC, MRI, NCAR, NCC, and UKMO Hadley Centre. NR 84 TC 124 Z9 125 U1 7 U2 72 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 18 PY 2012 VL 117 AR D14105 DI 10.1029/2011JD017237 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 977XN UT WOS:000306698300001 ER PT J AU Cornet, T Bourgeois, O Le Mouelic, S Rodriguez, S Sotin, C Barnes, JW Brown, RH Baines, KH Buratti, BJ Clark, RN Nicholson, PD AF Cornet, Thomas Bourgeois, Olivier Le Mouelic, Stephane Rodriguez, Sebastien Sotin, Christophe Barnes, Jason W. Brown, Robert H. Baines, Kevin H. Buratti, Bonnie J. Clark, Roger N. Nicholson, Phillip D. TI Edge detection applied to Cassini images reveals no measurable displacement of Ontario Lacus' margin between 2005 and 2010 SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ETOSHA PAN; TITAN; LAKES; EVOLUTION; NAMIBIA; ETHANE AB Ontario Lacus is thus far the largest flat-floored topographic depression of Titan's southern hemisphere interpreted as a permanent or ephemeral lake. From 2005 to 2010, it was imaged several times and at various wavelengths by ISS, VIMS and RADAR instruments onboard Cassini's spacecraft. We analyze the position and uncertainty of Ontario Lacus' margin in all these images using an edge detection method based on image derivation. We find that, given the range of uncertainties in contour locations derived from images, no measurable displacement of Ontario Lacus' margin can be detected between 2005 and 2010 at the actual image spatial resolutions. The discrepancy between this result and previous ones is attributable to differences in (1) the basics behind the methods used, (2) the actual spatial resolutions and contrasts of the available images due to differential atmospheric scattering effects at different wavelengths, and (3) the geomorphological interpretation of contours derived from images acquired at different wavelengths. This lack of measurable displacement in the images suggests that the imaged contour corresponds either (1) to the border of a surface liquid body, provided that potential changes in its extent over five terrestrial years were not sufficiently large to be measured, or (2) to the stationary topographic border between Ontario Lacus' depression and the surrounding alluvial plain. Potential displacements of Ontario Lacus' margin between 2005 and 2010 are thus below the actual resolution of currently available images or have to be sought for within the extent of the topographic depression rather than along its borders. C1 [Cornet, Thomas; Bourgeois, Olivier; Le Mouelic, Stephane; Sotin, Christophe] Univ Nantes, Lab Planetol & Geodynam Nantes, UMR 6112, F-44000 Nantes, France. [Cornet, Thomas; Bourgeois, Olivier; Le Mouelic, Stephane; Sotin, Christophe] CNRS, Nantes, France. [Cornet, Thomas; Bourgeois, Olivier; Le Mouelic, Stephane; Sotin, Christophe] OSUNA, Nantes, France. [Rodriguez, Sebastien] CEA Saclay, DSM, IRFU, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Sotin, Christophe; Baines, Kevin H.; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID USA. [Brown, Robert H.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Brown, Robert H.] Univ Arizona, Dept Astron, Tucson, AZ USA. [Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA. [Nicholson, Phillip D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Cornet, T (reprint author), Univ Nantes, Lab Planetol & Geodynam Nantes, UMR 6112, 2 Rue Houssiniere,BP92208, F-44000 Nantes, France. EM thomas.cornet@univ-nantes.fr RI Barnes, Jason/B-1284-2009; Rodriguez, Sebastien/H-5902-2016; Cornet, Thomas/E-7539-2017 OI Barnes, Jason/0000-0002-7755-3530; Rodriguez, Sebastien/0000-0003-1219-0641; Cornet, Thomas/0000-0001-5971-0056 FU Centre National d'Etudes Spatiales (CNES, France); Institut National des Sciences de l'Univers (INSU Programme National de Planetologie, Programme Reliefs, France); Agence Nationale de la Recherche [ANR-07-BLAN-0127]; NASA Astrobiology Institute FX The authors appreciate financial support provided by the Centre National d'Etudes Spatiales (CNES, France), the Institut National des Sciences de l'Univers (INSU Programme National de Planetologie, Programme Reliefs, France) and the Agence Nationale de la Recherche (project ANR-07-BLAN-0127 "Exoclimats," France). Part of this work has been performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. C.S. acknowledges support by NASA Astrobiology Institute. We thank Ellen Stofan and an anonymous reviewer for their effort in reviewing a preliminary version of the manuscript and for helping us clarify a number of important points. NR 37 TC 5 Z9 5 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUL 18 PY 2012 VL 117 AR E07005 DI 10.1029/2012JE004073 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 977YD UT WOS:000306700500002 ER PT J AU Plirdpring, T Kurosaki, K Kosuga, A Day, T Firdosy, S Ravi, V Snyder, GJ Harnwunggmoung, A Sugahara, T Ohishi, Y Muta, H Yamanaka, S AF Plirdpring, Theerayuth Kurosaki, Ken Kosuga, Atsuko Day, Tristan Firdosy, Samad Ravi, Vilupanur Snyder, G. Jeffrey Harnwunggmoung, Adul Sugahara, Tohru Ohishi, Yuji Muta, Hiroaki Yamanaka, Shinsuke TI Chalcopyrite CuGaTe2: A High-Efficiency Bulk Thermoelectric Material SO ADVANCED MATERIALS LA English DT Article DE thermoelectrics; chalcopyrite; CuGaTe2; thermal conductivity; electrical resistivity ID FIGURE-OF-MERIT; ELECTRICAL-PROPERTIES; THIN-FILMS; THERMAL-CONDUCTIVITY; TEMPERATURE-RANGE; CRYSTALS; CU; ENHANCEMENT; PERFORMANCE; CU2CDSNSE4 C1 [Plirdpring, Theerayuth; Kurosaki, Ken; Harnwunggmoung, Adul; Sugahara, Tohru; Ohishi, Yuji; Muta, Hiroaki; Yamanaka, Shinsuke] Osaka Univ, Grad Sch Engn, Suita, Osaka 5650871, Japan. [Plirdpring, Theerayuth; Harnwunggmoung, Adul] Rajamangala Univ Technol Suvarnabhumi, Fac Sci & Technol, Thermoelect & Nanotechnol Res Ctr, Huntra Phranakhon Si Ayu 13000, Thailand. [Kosuga, Atsuko] Osaka Prefecture Univ, Res Org 21st Century, Nanosci & Nanotechnol Res Ctr, Naka Ku, Sakai, Osaka 5998570, Japan. [Day, Tristan; Snyder, G. Jeffrey] CALTECH, Dept Mat Sci, Pasadena, CA 91125 USA. [Firdosy, Samad; Ravi, Vilupanur] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ravi, Vilupanur] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA. [Yamanaka, Shinsuke] Univ Fukui, Res Inst Nucl Engn, Fukui 9108507, Japan. RP Kurosaki, K (reprint author), Osaka Univ, Grad Sch Engn, 2-1 Yamadaoka, Suita, Osaka 5650871, Japan. EM kurosaki@see.eng.osaka-u.ac.jp RI Kurosaki, Ken/E-8081-2012; Snyder, G. Jeffrey/E-4453-2011; Snyder, G/I-2263-2015 OI Kurosaki, Ken/0000-0002-3015-3206; Snyder, G. Jeffrey/0000-0003-1414-8682; FU Ministry of Education, Culture, Sports, Science and Technology of Japan [21760519, 23686091]; Rajamangala University of Technology Suvarnabhumi; government of Thailand FX This work was supported in part by a Grant-in-Aid for Scientific Research (No. 21760519 & 23686091) from the Ministry of Education, Culture, Sports, Science and Technology of Japan. This work was also supported by the Rajamangala University of Technology Suvarnabhumi and the government of Thailand. NR 38 TC 106 Z9 108 U1 11 U2 169 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0935-9648 J9 ADV MATER JI Adv. Mater. PD JUL 17 PY 2012 VL 24 IS 27 BP 3622 EP 3626 DI 10.1002/adma.201200732 PG 5 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 971QJ UT WOS:000306218600003 PM 22689017 ER PT J AU Tatarov, B Muller, D Noh, YM Lee, KH Shin, DH Shin, SK Sugimoto, N Seifert, P Kim, YJ AF Tatarov, B. Mueller, D. Noh, Y. -M. Lee, K. -H. Shin, D. -H. Shin, S. -K. Sugimoto, N. Seifert, P. Kim, Y. -J. TI Record heavy mineral dust outbreaks over Korea in 2010: Two cases observed with multiwavelength aerosol/depolarization/Raman-quartz lidar SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ASIAN DUST; SAHARAN DUST; SAMUM 2006; EAST-ASIA; AEROSOL; DEPOLARIZATION; MOROCCO; RATIO; MODEL AB We report on two strong events of transport of mineral dust from Central Asia across Korea. The events took place in March and November 2010. The November case is important as fall is not a typical time for strong dust outbreaks in East Asia. We observed the dust with a multiwavelength aerosol/depolarization/Raman quartz lidar. The record PM-10 concentration of nearly 1600 mu g/m(3) in March 2010 exceeds the record value of 1470 mu g/m(3) measured in Seoul in March 2002. The event in November was the strongest case of dust transport ever observed over Korea in fall. We find up to 360 mu g/m(3) dust in heights above 250 m which is significantly different from the ground-based PM-10 observations. Citation: Tatarov, B., D. Muller, Y.-M. Noh, K.-H. Lee, D.-H. Shin, S.-K. Shin, N. Sugimoto, P. Seifert, and Y.-J. Kim (2012), Record heavy mineral dust outbreaks over Korea in 2010: Two cases observed with multiwavelength aerosol/depolarization/Raman-quartz lidar, Geophys. Res. Lett., 39, L14801, doi:10.1029/2012GL051972. C1 [Mueller, D.] NASA, Sci Syst & Applicat Inc, Langley Res Ctr, Hampton, VA 23681 USA. [Tatarov, B.; Mueller, D.; Noh, Y. -M.; Shin, D. -H.; Shin, S. -K.; Kim, Y. -J.] Gwangju Inst Sci & Technol, Atmospher Remote Sensing Lab, Kwangju, South Korea. [Mueller, D.; Seifert, P.] Leibniz Inst Tropospher Res, Leipzig, Germany. [Lee, K. -H.] Kyungil Univ, Dept Satellite Geoinformat Engn, Gyongsan, South Korea. [Sugimoto, N.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. RP Muller, D (reprint author), NASA, Sci Syst & Applicat Inc, Langley Res Ctr, MS 475, Hampton, VA 23681 USA. EM detlef@tropos.de RI Sugimoto, Nobuo/C-5189-2015; Seifert, Patric/D-2448-2014; MUELLER, DETLEF/F-1010-2015 OI Lee, Kwon-Ho/0000-0002-0844-5245; Sugimoto, Nobuo/0000-0002-0545-1316; Seifert, Patric/0000-0002-5626-3761; MUELLER, DETLEF/0000-0002-0203-7654 FU Korea Meteorological Administration Research and Development Program [CATER 2012-7080] FX This work was funded by the Korea Meteorological Administration Research and Development Program under grant CATER 2012-7080. The authors gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model and/or READY website (http://www.arl.noaa.gov/ready.php). NR 22 TC 6 Z9 7 U1 2 U2 12 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 JUL 17 PY 2012 VL 39 AR L14801 DI 10.1029/2012GL051972 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 977XZ UT WOS:000306700000001 ER PT J AU Hall, DK Comiso, JC DiGirolamo, NE Shuman, CA Key, JR Koenig, LS AF Hall, Dorothy K. Comiso, Josefino C. DiGirolamo, Nicol E. Shuman, Christopher A. Key, Jeffrey R. Koenig, Lora S. TI A Satellite-Derived Climate-Quality Data Record of the Clear-Sky Surface Temperature of the Greenland Ice Sheet SO JOURNAL OF CLIMATE LA English DT Article ID POLAR PATHFINDER DATASET; ARCTIC SURFACE; RADIATION PROPERTIES; CLOUD DETECTION; MASS-LOSS; ABLATION ZONE; RECENT TRENDS; PART II; MODIS; MELT AB The authors have developed a climate-quality data record of the clear-sky surface temperature of the Greenland Ice Sheet using the Moderate-Resolution Imaging Spectroradiometer (MODIS) ice-surface temperature (IST) algorithm. Daily and monthly quality-controlled MODIS ISTs of the Greenland Ice Sheet beginning on 1 March 2000 and continuing through 31 December 2010 are presented at 6.25-km spatial resolution on a polar stereographic grid along with metadata to permit detailed accuracy assessment. The ultimate goal is to develop a climate data record (CDR) that starts in 1981 with the Advanced Very High Resolution Radiometer (AVHRR) Polar Pathfinder (APP) dataset and continues with MOD IS data from 2000 to the present, and into the Visible Infrared Imager Radiometer Suite (VIIRS) era (the first VIIRS instrument was launched in October 2011). Differences in the APP and MODIS cloud masks have thus far precluded merging the APP and MODIS IST records, though this will be revisited after the APP dataset has been reprocessed with an improved cloud mask. IST of Greenland may be used to study temperature and melt trends and may also be used in data assimilation modeling and to calculate ice sheet mass balance. The MODIS IST climate-quality dataset provides a highly consistent and well-characterized record suitable for merging with earlier and future IST data records for climate studies. The complete MODIS IST daily and monthly data record is available online. C1 [Hall, Dorothy K.; Comiso, Josefino C.; Koenig, Lora S.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [DiGirolamo, Nicol E.] SSAI, Lanham, MD USA. [Shuman, Christopher A.] UMBC JCET, Baltimore, MD USA. [Key, Jeffrey R.] NOAA, Ctr Satellite Applicat & Res, NESDIS, Madison, WI USA. RP Hall, DK (reprint author), NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA. EM dorothy.k.hall@nasa.gov RI Key, Jeffrey/F-5597-2010 OI Key, Jeffrey/0000-0001-6109-3050 FU NASA FX The authors thank the following people for valuable suggestions during the course of this work: Chuck Fowler (NSIDC), George Riggs (SSAI & NASA/GSFC), and Xuanji Wang (University of Wisconsin/CIMSS). The authors would like to acknowledge Michiel van den Broeke from Utrecht University, The Netherlands, for providing automatic-weather station data for comparison with the MODIS-derived ice-surface temperatures. The NASA Cryospheric Sciences Program provided funding for the parts of this work performed at NASA/GSFC. The views, opinions, and findings contained in this report are those of the author(s) and should not be construed as an official NASA, National Oceanic and Atmospheric Administration, or U.S. Government position, policy, or decision. NR 46 TC 22 Z9 23 U1 1 U2 16 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 JUL 15 PY 2012 VL 25 IS 14 BP 4785 EP 4798 DI 10.1175/JCLI-D-11-00365.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 982FI UT WOS:000307027800002 ER PT J AU Ham, YG Schubert, S Chang, YH AF Ham, Yoo-Geun Schubert, Siegfried Chang, Yehui TI Optimal Initial Perturbations for Ensemble Prediction of the Madden-Julian Oscillation during Boreal Winter SO JOURNAL OF CLIMATE LA English DT Article ID SINGULAR VECTOR ANALYSIS; STATISTICAL FORECAST MODEL; GENERAL-CIRCULATION MODELS; INTRASEASONAL OSCILLATIONS; TROPICAL PACIFIC; OPTIMAL-GROWTH; COUPLED MODEL; EL-NINO; PREDICTABILITY; ENSO AB An initialization strategy, tailored to the prediction of the Madden-Julian oscillation (MJO), is evaluated using the Goddard Earth Observing System Model, version 5 (GEOS-5), coupled general circulation model (CGCM). The approach is based on the empirical singular vectors (ESVs) of a reduced-space statistically determined linear approximation of the full nonlinear CGCM. The initial ESV, extracted using 10 years (1990-99) of boreal winter hindcast data, has zonal wind anomalies over the western Indian Ocean, while the final ESV (at a forecast lead time of 10 days) reflects a propagation of the zonal wind anomalies to the east over the Maritime Continent-an evolution that is characteristic of the MJO. A new set of ensemble hindcasts are produced for the boreal winter season from 1990 to 1999 in which the leading ESV provides the initial perturbations. The results are compared with those from a set of control hindcasts generated using random perturbations. It is shown that the ESV-based predictions have a systematically higher bivariate correlation skill in predicting the MJO compared to those using the random perturbations. Furthermore, the improvement in the skill depends on the phase of the MJO. The ESV is particularly effective in increasing the forecast skill during those phases of the MJO in which the control has low skill (with correlations increasing by as much as 0.2 at 20-25-day lead times), as well as during those times in which the MJO is weak. C1 [Ham, Yoo-Geun; Schubert, Siegfried] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Ham, Yoo-Geun] Univ Space Res Assoc, Greenbelt, MD USA. [Chang, Yehui] Morgan State Univ, Baltimore, MD 21239 USA. [Chang, Yehui] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Baltimore, MD USA. RP Ham, YG (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20770 USA. EM yoo-geun.ham@nasa.gov FU NOAA Modeling, Analysis, Predictions, and Projections (MAPP) program; NASA Modeling, Analysis and Prediction (MAP) program FX Support for this project was provided by the NOAA Modeling, Analysis, Predictions, and Projections (MAPP) program and the NASA Modeling, Analysis and Prediction (MAP) program. NR 59 TC 6 Z9 7 U1 0 U2 4 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 JUL 15 PY 2012 VL 25 IS 14 BP 4932 EP 4945 DI 10.1175/JCLI-D-11-00344.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 982FI UT WOS:000307027800010 ER PT J AU Yao, MS Cheng, Y AF Yao, Mao-Sung Cheng, Ye TI Cloud Simulations in Response to Turbulence Parameterizations in the GISS Model E GCM SO JOURNAL OF CLIMATE LA English DT Article ID COMMUNITY ATMOSPHERE MODEL; BOUNDARY-LAYER; CLIMATE MODELS; CLOSURE-MODEL; CONVECTION; PROJECT; ECMWF; PBL AB The response of cloud simulations to turbulence parameterizations is studied systematically using the GISS general circulation model (GCM) E2 employed in the Intergovernmental Panel on Climate Change's (IPCC) Fifth Assessment Report (AR5). Without the turbulence parameterization, the relative humidity (RH) and the low cloud cover peak unrealistically close to the surface; with the dry convection or with only the local turbulence parameterization, these two quantities improve their vertical structures, but the vertical transport of water vapor is still weak in the planetary boundary layers (PBLs); with both local and nonlocal turbulence parameterizations, the RH and low cloud cover have better vertical structures in all latitudes due to more significant vertical transport of water vapor in the PBL. The study also compares the cloud and radiation climatologies obtained from an experiment using a newer version of turbulence parameterization being developed at GISS with those obtained from the AR5 version. This newer scheme differs from the AR5 version in computing nonlocal transports, turbulent length scale, and PBL height and shows significant improvements in cloud and radiation simulations, especially over the subtropical eastern oceans and the southern oceans. The diagnosed PBL heights appear to correlate well with the low cloud distribution over oceans. This suggests that a cloud-producing scheme needs to be constructed in a framework that also takes the turbulence into consideration. C1 [Yao, Mao-Sung; Cheng, Ye] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Yao, Mao-Sung] Sigma Space Partners LLC, New York, NY USA. [Cheng, Ye] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. RP Yao, MS (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mao-sung.yao@nasa.gov FU NASA's Modeling, Analysis and Prediction Program FX We thank A. Del Genio for critically reviewing the manuscript and for his many useful suggestions, and J. Wu for analyzing the diurnal variations of the convective precipitation. We also thank the two anonymous reviewers for their helpful suggestions that made this manuscript possible. This study is supported by NASA's Modeling, Analysis and Prediction Program. NR 29 TC 15 Z9 15 U1 1 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL 15 PY 2012 VL 25 IS 14 BP 4963 EP 4974 DI 10.1175/JCLI-D-11-00399.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 982FI UT WOS:000307027800012 ER PT J AU Ham, YG Kug, JS Lim, MJ AF Ham, Yoo-Geun Kug, Jong-Seong Lim, Mi-Jung TI Rectification Feedback of High-Frequency Atmospheric Variability into Low-Frequency Zonal Flows in the Tropical Pacific SO JOURNAL OF CLIMATE LA English DT Article ID WESTERLY WIND BURSTS; MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODEL; SEA-SURFACE TEMPERATURE; EL-NINO EVENTS; SYNOPTIC-SCALE DISTURBANCES; INTRASEASONAL VARIABILITY; EQUATORIAL PACIFIC; COUPLED GCM; GLOBAL PRECIPITATION AB In this study, the rectification process of high-frequency (HF) zonal-wind variability on the low-frequency (LF) zonal wind is investigated through an idealized experiment using an atmospheric general circulation model (AGCM). Through an idealized AGCM experiment with a fixed SST boundary forcing, it is shown that there is positive (negative) correlation between HF (2-90-day period) zonal-wind variance and LF (3-month average) zonal wind where the HF zonal-wind variance is positively (negatively) skewed because the stronger HF westerly (easterly) wind events than HF easterly (westerly) wind events induce a residual westerly (easterly), and it results in an additional rectified LF westerly (easterly) anomaly. This means that, over regions with positively skewed HF zonal winds, LF westerly anomalies are generated due to the residuals of the HF zonal winds. It implies that the LF zonal wind can be generated through internal processes of the atmosphere without external forcing and the interaction between LF and HF is not a one-way process from LF to HF but, rather, a two-way interaction process. C1 [Kug, Jong-Seong] Korea Ocean Res & Dev Inst, Ansan 435600, South Korea. [Lim, Mi-Jung] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. [Ham, Yoo-Geun] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA. [Ham, Yoo-Geun] Univ Space Res Assoc, Columbia, MD USA. RP Kug, JS (reprint author), Korea Ocean Res & Dev Inst, Ansan 435600, South Korea. EM jskug@kordi.re.kr RI KUG, JONG-SEONG/A-8053-2013 FU National Research Foundation of Korea [NRF-2009-C1AAA001-2009-0093042]; Korean government (MEST) FX This work was supported by the National Research Foundation of Korea (Grant NRF-2009-C1AAA001-2009-0093042), funded by the Korean government (MEST). NR 81 TC 1 Z9 1 U1 0 U2 4 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 JUL 15 PY 2012 VL 25 IS 14 BP 5088 EP 5101 DI 10.1175/JCLI-D-11-00303.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 982FI UT WOS:000307027800020 ER PT J AU Wu, LL Druschel, G Findlay, A Beard, BL Johnson, CM AF Wu, Lingling Druschel, Greg Findlay, Alyssa Beard, Brian L. Johnson, Clark M. TI Experimental determination of iron isotope fractionations among Fe-aq(2+)-FeSaq-Mackinawite at low temperatures: Implications for the rock record SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID DENSITY-FUNCTIONAL THEORY; 125 DEGREES-C; PYRITE FORMATION; AQUEOUS-SOLUTIONS; HYDROGEN-SULFIDE; NANOPARTICULATE MACKINAWITE; STABILITY-CONSTANTS; CLUSTER COMPLEXES; NATURAL-WATERS; II MONOSULFIDE AB The Fe isotope fractionation factors among aqueous ferrous iron (Fe-aq(2+)), aqueous FeS clusters (FeSaq), and nanoparticulate mackinawite under neutral and mildly acidic and alkaline pH conditions have been determined using the three-isotope method. Combined voltammetric analysis and geochemical modeling were used to determine the Fe speciation in the experimental systems. The equilibrium Fe-56/Fe-54 fractionation factor at 20 degrees C and pH 7 has been determined to be -0.32 +/- 0.29 (2 sigma)parts per thousand between Fe-aq(2+) (minor FeSaq also present in the experiment) and mackinawite. This fractionation factor was essentially constant when pH was changed to 6 or 8. When equal molarity of HS- and Fe-aq(2+) were added to the system, however, the isotopic fractionation at pH 7 changed to -0.64 +/- 0.36 (2 sigma)parts per thousand, correlating with a significant increase in the proportion of FeHS+ and FeSaq. These results highlight a more important role of aqueous Fe-S speciation in the equilibrium Fe isotope fractionation factor than recognized in previous studies. The isotopic fractionation remained constant when temperature was increased from 20 degrees C to 35 degrees C for fractionation factors between Fe-aq(2+), and mackinawite and between dominantly FeHS+ and mackinawite. Synthesis experiments similar to those of Butler et al. (2005) and Guilbaud et al. (2010) at pH 4 show consistent results: over time, the aqueous Fe-mackinawite fractionation decreases but even after 38 days of aging the fractionation factor is far from the equilibrium value inferred using the three-isotope method. In contrast, at near-neutral pH the fractionation factor for the synthesis experiment reached the equilibrium value in 38 days. These differences are best explained by noting that at low pH the FeS mackinawite particles coarsen more rapidly via particle aggregation, which limits isotopic exchange, whereas at higher pH mackinawite aggregation is limited, and Fe isotope exchange occurs more rapidly, converging on the equilibrium value. These results suggest that mackinawite formed in natural environments at near-neutral or alkaline pH are unlikely to retain kinetic isotope fractionations, but are more likely to reflect equilibrium isotope compositions. This in turn has important implications for interpreting iron isotope compositions of Fe sulfides in natural systems. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Wu, Lingling; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Wu, Lingling; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. [Druschel, Greg; Findlay, Alyssa] Univ Vermont, Dept Geol, Burlington, VT 05405 USA. [Druschel, Greg] Indiana Univ Purdue Univ, Dept Earth Sci, Indianapolis, IN 46202 USA. RP Wu, LL (reprint author), Univ Waterloo, Dept Earth & Environm Sci, Waterloo, ON N2L 3G1, Canada. EM lingling.wu@uwaterloo.ca RI Wu, Lingling/E-4087-2010 OI Wu, Lingling/0000-0002-8211-5754 FU National Science Foundation [EAR-0635593, EAR-0635523, EAR 0955639, ACS-PRF 43356-GB2] FX This work was supported by National Science Foundation grant EAR-0635593 (Johnson and Beard), EAR-0635523 (Druschel), EAR 0955639 (Druschel), and ACS-PRF 43356-GB2 (Druschel). Druschel gratefully acknowledges the work of several students who assisted with different parts of the lab work at the University of Vermont, including Harry Oduro, Jessica Sperling, and Christine Cramer. We thank AE D. Vance and three anonymous reviewers for helpful comments on the manuscript. NR 74 TC 17 Z9 19 U1 1 U2 42 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 JUL 15 PY 2012 VL 89 BP 46 EP 61 DI 10.1016/j.gca.2012.04.047 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 959SU UT WOS:000305334100004 ER PT J AU Drouin, BJ Gupta, H Yu, SS Miller, CE Muller, HSP AF Drouin, Brian J. Gupta, Harshal Yu, Shanshan Miller, Charles E. Mueller, Holger S. P. TI High resolution spectral analysis of oxygen. II. Rotational spectra of a(1)Delta(g) O-2 isotopologues SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MAGNETIC HYPERFINE-STRUCTURE; ORBITAL G-FACTOR; MOLECULAR-OXYGEN; GROUND-STATE; RESONANCE-SPECTRUM; CARBON-MONOXIDE; WAVE SPECTRUM; TRANSITIONS; CONSTANTS; SPECTROSCOPY AB As part of a comprehensive review on molecular oxygen spectroscopy, we have measured rotational spectra of isotopic forms of molecular oxygen in its a(1)Delta(g) electronic state with high-resolution terahertz spectroscopy. The data are recorded in close proximity to predicted positions. Due to the high resolution and good signal-to-noise ratio, the fundamental hyperfine parameters eQq and CI are determinable for O-17-substituted species for the first time. A refined nuclear spin orbit coupling constant, a = -211.9328(283) MHz, was determined, and is roughly two orders of magnitude more precise than values determined from near infrared spectroscopy or electron spin resonance studies. Vibrationally excited oxygen in the a(1)Delta(g) electronic state was also observable with small signal levels for many of the rotational transitions. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4719169] C1 [Drouin, Brian J.; Gupta, Harshal; Yu, Shanshan; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mueller, Holger S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. 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 Bundesministerium fur Bildung und Forschung (BMBF); Deutsche Forschungs Gemeinschaft (DFG) [SFB 494] FX This paper presents research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. H. S. P. M. is very grateful to the Bundesministerium fur Bildung und Forschung (BMBF) for financial support aimed at maintaining the Cologne Database for Molecular Spectroscopy, CDMS. The BMBF is administered by the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). A large portion of the work in Cologne was supported by the Deutsche Forschungs Gemeinschaft (DFG) in the framework of the collaborative research grant SFB 494. Additional support by the Land Nordrhein-Westfalen (NRW) is also acknowledged. Government sponsorship is acknowledged. NR 44 TC 7 Z9 7 U1 0 U2 16 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 14 PY 2012 VL 137 IS 2 AR 024305 DI 10.1063/1.4719169 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 973LG UT WOS:000306361000015 PM 22803534 ER PT J AU Yu, SS Miller, CE Drouin, BJ Muller, HSP AF Yu, Shanshan Miller, Charles E. Drouin, Brian J. Mueller, Holger S. P. TI High resolution spectral analysis of oxygen. I. Isotopically invariant Dunham fit for the X-3 Sigma(-)(g), a(1)Delta(g), b(1)Sigma(+)(g) states SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SCHUMANN-RUNGE BANDS; SUBMILLIMETER-WAVE SPECTRUM; ATMOSPHERIC ABSORPTION-BANDS; ROTATIONAL RAMAN-SPECTRA; RING-DOWN SPECTROSCOPY; INTRACAVITY LASER SPECTROSCOPY; FOURIER-TRANSFORM SPECTROSCOPY; MAGNETIC-DIPOLE TRANSITIONS; MOLECULAR-OXYGEN; GROUND-STATE AB We have developed a simultaneous global fit to the MW, THz, infrared, visible, and UV transitions of all six oxygen isotopologues, (OO)-O-16-O-16, (OO)-O-16-O-17, (OO)-O-16-O-18, (OO)-O-17-O-17, (OO)-O-17-O-18, (OO)-O-18-O-18, with the objective of predicting all transitions below the O(P-3) + O(P-3) dissociation threshold as well as the B-3 Sigma(+)(u) state from O(P-3)+O(D-1) within state-of-the-art experimental uncertainty. Here, we report an isotopically invariant Dunham fit for the lowest three electronic states, X-3 Sigma(-)(g), a(1)Delta(g), and b(1)Sigma(+)(g). Experimental transition frequencies involving these three states of all six O-2 isotopologues were critically reviewed and incorporated into the analysis. For the (OO)-O-16-O-16 isotopologue, experimental data sample vibrational states upsilon = 0-31 for X-3 Sigma(-)(g), upsilon = 0-10 for a(1)Delta(g), and upsilon = 0-12 for b(1)Sigma(+)(g). To the best of our knowledge, this is the first analysis that simultaneously fits spectra from all six O-2 isotopologues. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4719170] C1 [Yu, Shanshan; Miller, Charles E.; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mueller, Holger S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Yu, SS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shanshan.yu@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU National Aeronautics and Space Administration (NASA); Bundesministerium fur Bildung und Forschung (BMBF) FX 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 (NASA). We would like to thank the reviewers for useful comments. S. Y. would like to thank T. Slanger for providing unpublished data on the Chamberlain system, M. Ginter and his wife for their efforts to look for unpublished Schumann-Runge data, I. Gordon for providing his 16O18O. band data before his publication, R. Jongma for providing his unpublished data involving the X3Sigmag - state upsilon = 26-31. H. S. P. M. is very grateful to the Bundesministerium fur Bildung und Forschung (BMBF) for financial support aimed at maintaining the Cologne Database for Molecular Spectroscopy, CDMS. This support has been administered by the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). NR 132 TC 22 Z9 22 U1 0 U2 31 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 14 PY 2012 VL 137 IS 2 AR 024304 DI 10.1063/1.4719170 PG 20 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 973LG UT WOS:000306361000014 PM 22803533 ER PT J AU Jung, HC Jasinski, M Kim, JW Shum, CK Bates, P Neal, J Lee, H Alsdorf, D AF Jung, Hahn Chul Jasinski, Michael Kim, Jin-Woo Shum, C. K. Bates, Paul Neal, Jeffrey Lee, Hyongki Alsdorf, Doug TI Calibration of two-dimensional floodplain modeling in the central Atchafalaya Basin Floodway System using SAR interferometry SO WATER RESOURCES RESEARCH LA English DT Article ID WATER-LEVEL CHANGES; RASTER-BASED MODEL; AMAZON FLOODPLAIN; RADAR INTERFEROMETRY; HYDRAULIC MODELS; LOUISIANA; SIMULATION; RESOLUTION; ALTIMETRY; STORAGE AB Two-dimensional (2-D) satellite imagery has been increasingly employed to improve prediction of floodplain inundation models. However, most focus has been on validation of inundation extent, with little attention on the spatial variations of water elevation and slope. The availability of high resolution Interferometric Synthetic Aperture Radar (InSAR) imagery offers unprecedented opportunity for quantitative validation of surface water heights and slopes derived from 2D hydrodynamic models. In this study, the LISFLOOD-ACC hydrodynamic model is applied to the central Atchafalaya Basin Floodway System, Louisiana, during high flows typical of spring floods in the Mississippi Delta region, for the purpose of demonstrating the utility of InSAR in 2-D floodplain model calibration. Two schemes calibrating Manning's roughness in channels and floodplains are compared. First, the model is calibrated in terms of water elevations at a single in situ gage during a 62-d simulation period from 1 April 2008 to 1 June 2008. Second, the model is calibrated in terms of water elevation changes calculated from ALOS PALSAR 2D imagery acquired on 16 April 2008 and 1 June 2009, an interval of 46 d. The best-fit model shows that the mean absolute error is 5.7 cm/46 d for InSAR water level calibration. Daily storage changes within the similar to 230-km(2) model area are also calculated to be on the order of 107 m(3) d(-1) during high water of the modeled period. The favorable comparison between both approaches demonstrates the feasibility of SAR interferometry for 2-D hydrodynamic model calibration and for improved understanding of complex floodplain hydrodynamics. C1 [Jung, Hahn Chul; Jasinski, Michael] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Kim, Jin-Woo; Shum, C. K.; Alsdorf, Doug] Ohio State Univ, Div Geodet Sci, Sch Earth Sci, Columbus, OH 43210 USA. [Bates, Paul; Neal, Jeffrey] Univ Bristol, Sch Geog Sci, Bristol, Avon, England. [Lee, Hyongki] Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA. RP Jung, HC (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Bldg 33,Greenbelt Rd, Greenbelt, MD 20771 USA. EM hahnchul.jung@nasa.gov RI Neal, Jeffrey/C-8723-2009; Bates, Paul/C-8026-2012 OI Neal, Jeffrey/0000-0001-5793-9594; Bates, Paul/0000-0001-9192-9963 FU Goddard Space Flight Center (GSFC); NASA; NASA's Hydrology Program; OSU's Climate, Water and Carbon Program FX This research was supported by an appointment to the NASA Postdoctoral Program (NPP) at the Goddard Space Flight Center (GSFC), administered by Oak Ridge Associated Universities (ORAU) through a contract with NASA. We acknowledge the NASA Center for Climate Simulation (NCCS) and the OH Supercomputer Center (OSC) for use of the computing resources. The Ohio State University (OSU) component of the research is partially supported by NASA's Hydrology Program and OSU's Climate, Water and Carbon Program. We thank Yvonne Allen in USACE for sharing her knowledge of the Atchafalaya Basin Floodway System. LiDAR data were undertaken and provided by U.S.G.S. National Geospatial Program and U.S.G.S. Coastal and Marine Geology Program. ALOS PALSAR data were provided by AK Satellite Facility (ASF). NR 67 TC 10 Z9 10 U1 0 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD JUL 13 PY 2012 VL 48 AR W07511 DI 10.1029/2012WR011951 PG 13 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 974WC UT WOS:000306467100002 ER PT J AU Steele, A McCubbin, FM Fries, M Kater, L Boctor, NZ Fogel, ML Conrad, PG Glamoclija, M Spencer, M Morrow, AL Hammond, MR Zare, RN Vicenzi, EP Siljestrom, S Bowden, R Herd, CDK Mysen, BO Shirey, SB Amundsen, HEF Treiman, AH Bullock, ES Jull, AJT AF Steele, A. McCubbin, F. M. Fries, M. Kater, L. Boctor, N. Z. Fogel, M. L. Conrad, P. G. Glamoclija, M. Spencer, M. Morrow, A. L. Hammond, M. R. Zare, R. N. Vicenzi, E. P. Siljestrom, S. Bowden, R. Herd, C. D. K. Mysen, B. O. Shirey, S. B. Amundsen, H. E. F. Treiman, A. H. Bullock, E. S. Jull, A. J. T. TI A Reduced Organic Carbon Component in Martian Basalts SO SCIENCE LA English DT Article ID ALLAN HILLS 84001; POLYCYCLIC AROMATIC-HYDROCARBONS; METEORITE ALH84001; ISOTOPIC EVIDENCE; OXYGEN FUGACITY; MARS; ORIGIN; MANTLE; GRAPHITE; IMPACT AB The source and nature of carbon on Mars have been a subject of intense speculation. We report the results of confocal Raman imaging spectroscopy on 11 martian meteorites, spanning about 4.2 billion years of martian history. Ten of the meteorites contain abiotic macromolecular carbon (MMC) phases detected in association with small oxide grains included within high-temperature minerals. Polycyclic aromatic hydrocarbons were detected along with MMC phases in Dar al Gani 476. The association of organic carbon within magmatic minerals indicates that martian magmas favored precipitation of reduced carbon species during crystallization. The ubiquitous distribution of abiotic organic carbon in martian igneous rocks is important for understanding the martian carbon cycle and has implications for future missions to detect possible past martian life. C1 [Steele, A.; McCubbin, F. M.; Boctor, N. Z.; Fogel, M. L.; Glamoclija, M.; Bowden, R.; Mysen, B. O.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [McCubbin, F. M.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Fries, M.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Kater, L.] Witec GmbH, D-89081 Ulm, Germany. [Conrad, P. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spencer, M.; Morrow, A. L.; Hammond, M. R.; Zare, R. N.] Stanford Univ, Dept Chem, Stanford, CA 94305 USA. [Vicenzi, E. P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Siljestrom, S.] Stockholm Univ, Dept Geol Sci, S-10691 Stockholm, Sweden. [Siljestrom, S.] SP Tech Res Inst Sweden, Dept Chem & Mat, S-50115 Boras, Sweden. [Herd, C. D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Shirey, S. B.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Amundsen, H. E. F.] Earth Explorat Serv, N-0364 Oslo, Norway. [Amundsen, H. E. F.] Planetary Explorat Serv, N-0364 Oslo, Norway. [Treiman, A. H.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Bullock, E. S.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Jull, A. J. T.] Univ Arizona, Tucson, AZ 85721 USA. RP Steele, A (reprint author), Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. EM asteele@ciw.edu RI Steele, Andrew/A-3573-2013; McCubbin, Francis/D-1698-2009; Fogel, Marilyn/M-2395-2015 OI Fogel, Marilyn/0000-0002-1176-3818 FU NASA Astrobiology Science and Technology for Exploring Planets [NNX09AB74G]; NASA Mars Fundamental Research Program [NNX08AN61G]; W. M. Keck Foundation [2007-6-29]; NASA Astrobiology Institute [NNA09DA81A]; Carnegie Institution of Washington; NASA Cosmochemistry [NNX11AG76G]; Natural Science and Engineering Research Council of Canada [261740] FX This work was funded by NASA Astrobiology Science and Technology for Exploring Planets (NNX09AB74G to A. S., P. G. C., A. H. T., and M. L. F.), NASA Mars Fundamental Research Program (NNX08AN61G to A. S.), the W. M. Keck Foundation (2007-6-29 to M. L. F. and A. S.), NASA Astrobiology Institute (NNA09DA81A to A. S., S. B. S., N.Z.B., B.O.M., and M. L. F.), and the Carnegie Institution of Washington. F. M. M. acknowledges financial support from NASA Cosmochemistry (NNX11AG76G to F. M. M.). A. S. thanks J. Strope for identification of suitable meteorite samples, C. Agee (University of New Mexico) for the Tissint sample, and L. Welzenbach, T. Gooding, and T. Rose for their assistance in thin-sectioning the meteorites and the use of the Scanning Electron Microscope in the Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC. C. D. K. H. thanks D. Hnatyshin for assistance with oxygen fugacity calculations. This work was supported by Natural Science and Engineering Research Council of Canada grant 261740 "The Geology of Mars from Studies of Martian Meteorites" to C. D. K. H. L2MS, 14C, and additional Raman data have been included in the supplementary materials. NR 38 TC 74 Z9 77 U1 6 U2 107 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 JUL 13 PY 2012 VL 337 IS 6091 BP 212 EP 215 DI 10.1126/science.1220715 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 973AN UT WOS:000306323500053 PM 22628557 ER PT J AU Shen, BW Tao, WK Lin, YL Laing, A AF Shen, Bo-Wen Tao, Wei-Kuo Lin, Yuh-Lang Laing, Arlene TI Genesis of twin tropical cyclones as revealed by a global mesoscale model: The role of mixed Rossby gravity waves SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODEL; COUPLED EQUATORIAL WAVES; NUMERICAL SIMULATIONS; ENERGY ACCUMULATION; WESTERN PACIFIC; CLIMATE MODEL; NWP SYSTEM; DIANA 1984; PART II AB In this study, it is proposed that twin tropical cyclones (TCs), Kesiny and 01A, in May 2002 formed in association with the scale interactions of three gyres that appeared as a convectively coupled mixed Rossby gravity (ccMRG) wave during an active phase of the Madden-Julian Oscillation (MJO). This is shown by analyzing observational data, including NCEP reanalysis data and METEOSAT 7 IR satellite imagery, and performing numerical simulations using a global mesoscale model. A 10-day control run is initialized at 0000 UTC 1 May 2002 with grid-scale condensation but no sub-grid cumulus parameterizations. The ccMRG wave was identified as encompassing two developing and one non-developing gyres, the first two of which intensified and evolved into the twin TCs. The control run is able to reproduce the evolution of the ccMRG wave and thus the formation of the twin TCs about two and five days in advance as well as their subsequent intensity evolution and movement within an 8-10 day period. Five additional 10-day sensitivity experiments with different model configurations are conducted to help understand the interaction of the three gyres, leading to the formation of the TCs. These experiments suggest the improved lead time in the control run may be attributed to the realistic simulation of the ccMRG wave with the following processes: (1) wave deepening (intensification) associated with a reduction in wavelength and/or the intensification of individual gyres, (2) poleward movement of gyres that may be associated with boundary layer processes, (3) realistic simulation of moist processes at regional scales in association with each of the gyres, and (4) the vertical phasing of low- and mid-level cyclonic circulations associated with a specific gyre. C1 [Shen, Bo-Wen; Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shen, Bo-Wen] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Lin, Yuh-Lang] N Carolina Agr & Tech State Univ, Dept Phys, Greensboro, NC USA. [Laing, Arlene] UCAR COMET, Boulder, CO USA. RP Shen, BW (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. EM bo-wen.shen-1@nasa.gov FU NASA Earth Science Technology Office (ESTO); Advanced Information Systems Technology (AIST) Program; Modeling, Analysis and Prediction (MAP) Program FX We would like to thank C. Schreck and two anonymous reviewers for their valuable suggestions, which have substantially improved the manuscript, and R. Anthes for his comments and encouragement. We are grateful for the support from the following organizations: the NASA Earth Science Technology Office (ESTO), the Advanced Information Systems Technology (AIST) Program, and the Modeling, Analysis and Prediction (MAP) Program. We would also like to thank Stephen Lang for proofreading this manuscript and K.-S. Kuo for preparing Figure 2. Acknowledgment is also made of the NASA High-End Computing (HEC) Program and of the NASA Advanced Supercomputing (NAS) division and NASA Center for Climate Simulation (NCCS) for the computer time used in this research. NR 66 TC 11 Z9 11 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 12 PY 2012 VL 117 AR D13114 DI 10.1029/2012JD017450 PG 28 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 974UO UT WOS:000306463100002 ER PT J AU Galvan, DA Komjathy, A Hickey, MP Stephens, P Snively, J Song, YT Butala, MD Mannucci, AJ AF Galvan, David A. Komjathy, Attila Hickey, Michael P. Stephens, Philip Snively, Jonathan Song, Y. Tony Butala, Mark D. Mannucci, Anthony J. TI Ionospheric signatures of Tohoku-Oki tsunami of March 11, 2011: Model comparisons near the epicenter SO RADIO SCIENCE LA English DT Article ID INTERNAL GRAVITY-WAVES; PACIFIC COAST; EARTHQUAKE; DISTURBANCES; OSCILLATIONS; ATMOSPHERE; DEPENDENCE AB We observe ionospheric perturbations caused by the Tohoku earthquake and tsunami of March 11, 2011. Perturbations near the epicenter were found in measurements of ionospheric total electron content (TEC) from 1198 GPS receivers in the Japanese GEONET network. For the first time for this event, we compare these observations with the estimated magnitude and speed of a tsunami-driven atmospheric gravity wave, using an atmosphere-ionosphere-coupling model and a tsunami model of sea-surface height, respectively. Traveling ionospheric disturbances (TIDs) were observed moving away from the epicenter at approximate speeds of 3400 m/s, 1000 m/s and 200-300 m/s, consistent with Rayleigh waves, acoustic waves, and gravity waves, respectively. We focus our analysis on gravity waves moving south and east of the epicenter, since tsunamis propagating in the deep ocean have been shown to produce gravity waves detectable in ionospheric TEC in the past. Observed southeastward gravity wave perturbations, seen similar to 60 min after the earthquake, are mostly between 0.5 to 1.5 TECU, representing up to similar to 5% of the background vertical TEC (VTEC). Comparisons of observed TID gravity waves with the modeled tsunami speed in the ocean and the predicted VTEC perturbation amplitudes from an atmosphere-ionosphere-coupling model show the measurements and models to be in close agreement. Due to the dense GPS network and high earthquake magnitude, these are the clearest observations to date of the effect of a major earthquake and tsunami on the ionosphere near the epicenter. Such observations from a future real-time GPS receiver network could be used to validate tsunami models, confirm the existence of a tsunami, or track its motion where in situ buoy data is not available. C1 [Galvan, David A.; Komjathy, Attila; Stephens, Philip; Song, Y. Tony; Butala, Mark D.; Mannucci, Anthony J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Hickey, Michael P.; Snively, Jonathan] Embry Riddle Aeronaut Univ, Daytona Beach, FL USA. RP Galvan, DA (reprint author), RAND Corp, 1776 Main St, Santa Monica, CA 90401 USA. EM davidgalvan@gmail.com FU John LaBrecque of NASA Headquarters; Earth Science and Interior NASA ROSES Grant [NNH07ZDA001N-ESI] FX The authors would like to thank John LaBrecque of NASA Headquarters and the Earth Science and Interior NASA ROSES Grant (NNH07ZDA001N-ESI), which made this research possible. RINEX files from the Japanese GEONET network were provided by the Geospatial Information Authority (GSI), a part of the Japanese Ministry of Land, Infrastructure, Transport and Tourism. Data analysis and tsunami modeling work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract to the National Aeronautics and Space Administration. Atmosphere-Ionosphere coupling modeling work was performed at Embry Riddle Aeronautical University. NR 33 TC 50 Z9 50 U1 3 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 J9 RADIO SCI JI Radio Sci. PD JUL 12 PY 2012 VL 47 AR RS4003 DI 10.1029/2012RS005023 PG 10 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 974XL UT WOS:000306470800001 ER PT J AU Cannon, KM Sutter, B Ming, DW Boynton, WV Quinn, R AF Cannon, K. M. Sutter, B. Ming, D. W. Boynton, W. V. Quinn, R. TI Perchlorate induced low temperature carbonate decomposition in the Mars Phoenix Thermal and Evolved Gas Analyzer (TEGA) SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SIMULATED MARTIAN CONDITIONS; LANDING SITE; DIFFRACTION; DEGRADATION; CALCITE; STEAM; SOIL AB Simulated Thermal Evolved Gas Analyzer (TEGA) analyses have shown that a CO2 release detected between 400 degrees C and 680 degrees C by the Phoenix Lander's TEGA instrument may have been caused by a reaction between calcium carbonate and hydrated magnesium perchlorate. In our experiments a CO2 release beginning at 385 +/- 12 degrees C was attributed to calcite reacting with water vapor and HCl gas from the dehydration and thermal decomposition of Mg-perchlorate. The release of CO2 is consistent with the TEGA detection of CO2 released between 400 and 680 degrees C, with the amount of CO2 increasing linearly with added perchlorate. X-ray diffraction (XRD) experiments confirmed CaCl2 formation from the reaction between calcite and HCl. These results have important implications for the Mars Science Laboratory (MSL) Curiosity rover. Heating soils may cause inorganic release of CO2; therefore, detection of organic fragments, not CO2 alone, should be used as definitive evidence for organics in Martian soils. Citation: Cannon, K. M., B. Sutter, D. W. Ming, W. V. Boynton, and R. Quinn (2012), Perchlorate induced low temperature carbonate decomposition in the Mars Phoenix Thermal and Evolved Gas Analyzer (TEGA), Geophys. Res. Lett., 39, L13203, doi:10.1029/2012GL051952. C1 [Cannon, K. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Sutter, B.] Jacobs ESCG, Houston, TX USA. [Ming, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Boynton, W. V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Quinn, R.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Cannon, KM (reprint author), Brown Univ, Dept Geol Sci, 134 Brook St,Box 1846, Providence, RI 02912 USA. EM kevin_cannon@brown.edu FU Lunar Planetary Institute; Mars Data Analysis Program [NNX10AQ22G]; NASA [NNX09AM93G] FX Funding for this work was provided by the Lunar Planetary Institute Summer 2010 Intern program to K. Cannon, by the Mars Data Analysis Program to B. Sutter, D. W. Ming, and W. V. Boynton (grant NNX10AQ22G), and by the NASA Astrobiology: Exobiology and Evolutionary Biology grant (NNX09AM93G) to R. Quinn. The authors would like to thank Ron Peterson and the two anonymous reviewers whose comments significantly improved this paper. NR 23 TC 10 Z9 10 U1 1 U2 33 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 11 PY 2012 VL 39 AR L13203 DI 10.1029/2012GL051952 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 974UV UT WOS:000306463800001 ER PT J AU Galley, CR Leibovich, AK Rothstein, IZ AF Galley, Chad R. Leibovich, Adam K. Rothstein, Ira Z. TI Galley, Leibovich, and Rothstein Reply SO PHYSICAL REVIEW LETTERS LA English DT Editorial Material C1 [Galley, Chad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Galley, Chad R.] CALTECH, Pasadena, CA 91125 USA. [Leibovich, Adam K.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA. [Rothstein, Ira Z.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Galley, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Rothstein, Ira/O-2747-2014 OI Rothstein, Ira/0000-0002-3374-4212 NR 3 TC 4 Z9 4 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 11 PY 2012 VL 109 IS 2 AR 029502 DI 10.1103/PhysRevLett.109.029502 PG 1 WC Physics, Multidisciplinary SC Physics GA 973BI UT WOS:000306325900019 ER PT J AU Hu, RY Cahoy, K Zuber, MT AF Hu, Renyu Cahoy, Kerri Zuber, Maria T. TI Mars atmospheric CO2 condensation above the north and south poles as revealed by radio occultation, climate sounder, and laser ranging observations SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN POLAR CAPS; GENERAL-CIRCULATION MODEL; CARBON-DIOXIDE CLOUDS; GLOBAL SURVEYOR; SEASONAL CAP; ICE CLOUDS; ALTIMETER; TES; TEMPERATURES; PRESSURE AB We study the condensation of CO2 in Mars' atmosphere using temperature profiles retrieved from radio occultation measurements from Mars Global Surveyor (MGS) as well as the climate sounding instrument onboard the Mars Reconnaissance Orbiter (MRO), and detection of reflective clouds by the MGS Mars Orbiter Laser Altimeter (MOLA). We find 11 events in 1999 where MGS temperature profiles indicate CO2 condensation and MOLA simultaneously detects reflective clouds. We thus provide causal evidence that MOLA non-ground returns are associated with CO2 condensation, which strongly indicates their nature being CO2 clouds. The MGS and MRO temperature profiles together reveal the seasonal expansion and shrinking of the area and the vertical extent of atmospheric saturation. The occurrence rate of atmospheric saturation is maximized at high latitudes in the middle of winter. The atmospheric saturation in the northern polar region exhibits more intense seasonal variation than in the southern polar region. In particular, a shrinking of saturation area and thickness from LS similar to 270 degrees to similar to 300 degrees in 2007 is found; this is probably related to a planet-encircling dust storm. Furthermore, we integrate the condensation area and the condensation occurrence rate to estimate cumulative masses of CO2 condensates deposited onto the northern and southern seasonal polar caps. The precipitation flux is approximated by the particle settling flux which is estimated using the impulse responses of MOLA filter channels. With our approach, the total atmospheric condensation mass can be estimated from these observational data sets with average particle size as the only free parameter. By comparison with the seasonal polar cap masses inferred from the time-varying gravity of Mars, our estimates indicate that the average condensate particle radius is 8-22 mu m in the northern hemisphere and 4-13 mu m in the southern hemisphere. Our multi-instrument data analysis provides new constraints on modeling the global climate of Mars. C1 [Hu, Renyu; Cahoy, Kerri; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Cahoy, Kerri] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hu, RY (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 54-1719,77 Massachusetts Ave, Cambridge, MA 02139 USA. EM hury@mit.edu FU Radio Science Gravity investigation of the NASA Mars Reconnaissance Orbiter mission; NASA Earth and Space Science Fellowship [NNX11AP47H] FX We thank Greg Neumann for providing MOLA non-ground return data, Peter Ford and Gordon Pettengill for insightful discussions about cloud formation on Mars, Tim Schofield and David Kass for discussions about the MCS data, Anthony Colaprete and Timothy Titus for careful review of the manuscript, and Francois Forget for discussions about the atmospheric condensation. This analysis was supported by the Radio Science Gravity investigation of the NASA Mars Reconnaissance Orbiter mission. RH was partly supported by the NASA Earth and Space Science Fellowship (NNX11AP47H). NR 66 TC 10 Z9 10 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUL 10 PY 2012 VL 117 AR E07002 DI 10.1029/2012JE004087 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 974UJ UT WOS:000306462600001 ER PT J AU Berthier, E Scambos, TA Shuman, CA AF Berthier, Etienne Scambos, Ted A. Shuman, Christopher A. TI Mass loss of Larsen B tributary glaciers (Antarctic Peninsula) unabated since 2002 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ICE SHELF COLLAPSE; ELEVATION; DISINTEGRATION; ACCELERATION; RETREAT AB Ice mass loss continues at a high rate among the large glacier tributaries of the Larsen B Ice Shelf following its disintegration in 2002. We evaluate recent mass loss by mapping elevation changes between 2006 and 2010/11 using differencing of digital elevation models (DEMs). The measurement accuracy of these elevation changes is confirmed by a 'null test', subtracting DEMs acquired within a few weeks. The overall 2006-2010/11 mass loss rate (9.0 +/- 2.1 Gt a(-1)) is similar to the 2001/02-2006 rate (8.8 +/- 1.6 Gt a(-1)), derived using DEM differencing and laser altimetry. This unchanged overall loss masks a varying pattern of thinning and ice loss for individual glacier basins. On Crane Glacier, the thinning pulse, initially greatest near the calving front, is now broadening and migrating upstream. The largest losses are now observed for the Hektoria/Green glacier basin, having increased by 33% since 2006. Our method has enabled us to resolve large residual uncertainties in the Larsen B sector and confirm its state of ongoing rapid mass loss. C1 [Berthier, Etienne] Univ Toulouse, LEGOS, CNRS, F-31400 Toulouse, France. [Scambos, Ted A.] Univ Colorado, CIRES, NSIDC, Boulder, CO 80309 USA. [Shuman, Christopher A.] NASA, Goddard Space Flight Ctr, JCET, UMBC, Greenbelt, MD 20771 USA. RP Berthier, E (reprint author), Univ Toulouse, LEGOS, CNRS, 14 Av Edouard Belin, F-31400 Toulouse, France. EM etienne.berthier@legos.obs-mip.fr RI Berthier, Etienne/B-8900-2009 OI Berthier, Etienne/0000-0001-5978-9155 FU CNES; PNTS; NSF-OPP; NASA [NNX10AR76G]; [ANR-09-SYSC-001]; [ANT-0732921] FX We thank G. Durand, B. Kulessa and four anonymous referees for their comments on earlier versions of the paper. EB acknowledges support from CNES (TOSCA and ISIS proposals), PNTS, and ANR-09-SYSC-001. TAS acknowledges support from NSF-OPP, ANT-0732921, and NASA NNX10AR76G grants. CAS was supported by grants from the NASA Cryospheric Sciences Program. SPOT5 HRS data were provided at no cost by CNES through the SPIRIT project. ASTER data were provided at no cost by NASA/USGS through the Global Land Ice Measurements from Space (GLIMS) project. NR 25 TC 36 Z9 36 U1 1 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 10 PY 2012 VL 39 AR L13501 DI 10.1029/2012GL051755 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 974UU UT WOS:000306463700001 ER PT J AU Magnotti, G Cutler, AD Danehy, PM AF Magnotti, Gaetano Cutler, Andrew D. Danehy, Paul M. TI Beam shaping for CARS measurements in turbulent environments SO APPLIED OPTICS LA English DT Article ID RAMAN-SCATTERING MEASUREMENTS; SUPERSONIC COMBUSTOR; SPECTROSCOPY; TEMPERATURE; BOXCARS AB This paper describes a new technique to mitigate the effect of beam steering on CARS measurements in turbulent, variable density environments. The new approach combines planar BOXCARS phase-matching with elliptical shaping of one of the beams to generate a signal robust to beam steering, while keeping the same spatial resolution. Numerical and experimental results are provided to demonstrate the effectiveness of this approach. One experiment investigates the effect of beam shaping in the presence of a controlled and well quantified displacement of the beams at the focal plane. Another experiment, more qualitative, proves the effectiveness of the technique in the presence of severe beam steering due to turbulence. (C) 2012 Optical Society of America C1 [Magnotti, Gaetano; Cutler, Andrew D.] George Washington Univ, MAE Dept, Newport News, VA 23602 USA. [Danehy, Paul M.] NASA Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. RP Magnotti, G (reprint author), George Washington Univ, MAE Dept, 1 Old Oyster Point Rd, Newport News, VA 23602 USA. EM gaetanomagnotti@gmail.com OI Magnotti, Gaetano/0000-0002-1723-5258 FU NASA [NNX07AC32A, NNX08AB31A] FX This work was supported by the NASA Fundamental Aeronautics Program, Hypersonics Focus under grants NNX07AC32A and NNX08AB31A (Technical monitors Paul Danehy and Richard Gaffney). The authors would like to thank L.G. Wilson for technical support in performing these experiments. NR 30 TC 3 Z9 3 U1 0 U2 15 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JUL 10 PY 2012 VL 51 IS 20 BP 4730 EP 4741 DI 10.1364/AO.51.004730 PG 12 WC Optics SC Optics GA 972QB UT WOS:000306291100021 PM 22781249 ER PT J AU Jones, LW Courneya, KS Mackey, JR Muss, HB Pituskin, EN Scott, JM Hornsby, WE Coan, AD Herndon, JE Douglas, PS Haykowsky, M AF Jones, Lee W. Courneya, Kerry S. Mackey, John R. Muss, Hyman B. Pituskin, Edith N. Scott, Jessica M. Hornsby, Whitney E. Coan, April D. Herndon, James E., II Douglas, Pamela S. Haykowsky, Mark TI Cardiopulmonary Function and Age-Related Decline Across the Breast Cancer Survivorship Continuum SO JOURNAL OF CLINICAL ONCOLOGY LA English DT Article ID RANDOMIZED CONTROLLED-TRIAL; CONGESTIVE-HEART-FAILURE; CARDIAC REHABILITATION; CARDIOVASCULAR-DISEASE; ADJUVANT TRASTUZUMAB; OXYGEN-CONSUMPTION; RISK PROFILE; LUNG-CANCER; EXERCISE; WOMEN AB Purpose To evaluate cardiopulmonary function (as measured by peak oxygen consumption [VO2peak]) across the breast cancer continuum and its prognostic significance in women with metastatic disease. Patients and Methods Patients with breast cancer representing four cross-sectional cohorts-that is, (1) before, (2) during, and (3) after adjuvant therapy for nonmetastatic disease, and (4) during therapy in metastatic disease-were studied. A cardiopulmonary exercise test (CPET) with expired gas analysis was used to assess VO2peak. A Cox proportional hazards model was used to estimate the risk of death according to VO2peak category (< 15.4 v >= 15.4 mL . kg(-1) . min(-1)) with adjustment for clinical factors. Results A total of 248 women (age, 55 +/- 8 years) completed a CPET. Mean VO2peak was 17.8 +/- a standard deviation of 4.3 mL . kg(-1) . min(-1), the equivalent of 27% +/- 17% below age-matched healthy sedentary women. For the entire cohort, 32% had a VO2peak less than 15.4 mL . kg(-1) . min(-1)-the VO2peak required for functional independence. VO2peak was significantly different across breast cancer cohorts for relative (mL . kg(-1) . min(-1)) and absolute (L . min(-1)) VO2peak (P = .017 and P < .001, respectively); VO2peak was lowest in women with metastatic disease. In patients with metastatic disease (n = 52), compared with patients achieving a VO2peak <= 1.09 L . min(-1), the adjusted hazard ratio for death was 0.32 (95% CI, 0.16 to 0.67, P = .002) for a VO2peak more than 1.09 L . min(-1). Conclusion Patients with breast cancer have marked impairment in VO2peak across the entire survivorship continuum. VO2peak may be an independent predictor of survival in metastatic disease. C1 [Jones, Lee W.; Hornsby, Whitney E.; Coan, April D.; Herndon, James E., II; Douglas, Pamela S.] Duke Univ, Med Ctr, Durham, NC 27706 USA. [Muss, Hyman B.] Univ N Carolina, Chapel Hill, NC USA. [Courneya, Kerry S.; Mackey, John R.; Pituskin, Edith N.; Haykowsky, Mark] Univ Alberta, Edmonton, AB, Canada. [Scott, Jessica M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Jones, LW (reprint author), Duke Canc Inst, Box 3085, Durham, NC 27710 USA. EM lee.w.jones@duke.edu OI Sykes, April/0000-0002-7667-8155 FU National Institutes of Health [CA143254, CA142566, CA138634, CA133895, CA125458]; Canada Research Chairs Program FX Supported by National Institutes of Health Grants No. CA143254, CA142566, CA138634, CA133895, and CA125458 and funds from George and Susan Beischer (L.W.J.). K. S. C. is supported by the Canada Research Chairs Program. NR 42 TC 80 Z9 81 U1 0 U2 9 PU AMER SOC CLINICAL ONCOLOGY PI ALEXANDRIA PA 2318 MILL ROAD, STE 800, ALEXANDRIA, VA 22314 USA SN 0732-183X EI 1527-7755 J9 J CLIN ONCOL JI J. Clin. Oncol. PD JUL 10 PY 2012 VL 30 IS 20 BP 2530 EP 2537 DI 10.1200/JCO.2011.39.9014 PG 8 WC Oncology SC Oncology GA 971YU UT WOS:000306244300020 PM 22614980 ER PT J AU Abdo, AA Abeysekara, U Allen, BT Aune, T Berley, D Bonamente, E Christopher, GE DeYoung, T Dingus, BL Ellsworth, RW Galbraith-Frew, JG Gonzalez, MM Goodman, JA Hoffman, CM Huntemeyer, PH Hui, CM Kolterman, BE Linnemann, JT McEnery, JE Mincer, AI Morgan, T Nemethy, P Pretz, J Ryan, JM Parkinson, PMS Shoup, A Sinnis, G Smith, AJ Vasileiou, V Walker, GP Williams, DA Yodh, B AF Abdo, A. A. Abeysekara, U. Allen, B. T. Aune, T. Berley, D. Bonamente, E. Christopher, G. E. DeYoung, T. Dingus, B. L. Ellsworth, R. W. Galbraith-Frew, J. G. Gonzalez, M. M. Goodman, J. A. Hoffman, C. M. Huentemeyer, P. H. Hui, C. M. Kolterman, B. E. Linnemann, J. T. McEnery, J. E. Mincer, A. I. Morgan, T. Nemethy, P. Pretz, J. Ryan, J. M. Parkinson, P. M. Saz Shoup, A. Sinnis, G. Smith, A. J. Vasileiou, V. Walker, G. P. Williams, D. A. Yodh, B. TI SPECTRUM AND MORPHOLOGY OF THE TWO BRIGHTEST MILAGRO SOURCES IN THE CYGNUS REGION: MGRO J2019+37 AND MGRO J2031+41 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; astroparticle physics; gamma rays: general; open clusters and associations: individual (Cyg OB1, Cyg OB2); pulsars: general ID GAMMA-RAY EMISSION; SOURCE TEV J2032+4130; GALACTIC PLANE; CRAB-NEBULA; SOURCE LIST; PROPAGATION; FERMI; GALAXY AB The Cygnus region is a very bright and complex portion of the TeV sky, host to unidentified sources and a diffuse excess with respect to conventional cosmic-ray propagation models. Two of the brightest TeV sources, MGRO J2019+37 and MGRO J2031+41, are analyzed using Milagro data with a new technique, and their emission is tested under two different spectral assumptions: a power law and a power law with an exponential cutoff. The new analysis technique is based on an energy estimator that uses the fraction of photomultiplier tubes in the observatory that detect the extensive air shower. The photon spectrum is measured in the range 1-100 TeV using the last three years of Milagro data (2005-2008), with the detector in its final configuration. An F-test indicates that MGRO J2019+37 is better fit by a power law with an exponential cutoff than by a simple power law. The best-fitting parameters for the power law with exponential cutoff model are a normalization at 10 TeV of 7(-2)(+5) x 10(-10) s(-1) m(-2) TeV-1, a spectral index of 2.0(-1.0)(+0.5), and a cutoff energy of 29(-16)(+50) TeV. MGRO J2031+41 shows no evidence of a cutoff. The best-fitting parameters for a power law are a normalization of 2.1(-0.6)(+0.6)x10 (10) s (1) m (2) TeV (1) and a spectral index of 3.22(-0.18)(+0.23). The overall flux is subject to a similar to 30% systematic uncertainty. The systematic uncertainty on the power-law indices is similar to 0.1. Both uncertainties have been verified with cosmic-ray data. A comparison with previous results from TeV J2032+4130, MGRO J2031+41, and MGRO J2019+37 is also presented. C1 [Abdo, A. A.; Abeysekara, U.; Linnemann, J. T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Allen, B. T.; Yodh, B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Aune, T.; Parkinson, P. M. Saz; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Berley, D.; Goodman, J. A.; Smith, A. J.; Vasileiou, V.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bonamente, E.; Galbraith-Frew, J. G.; Huentemeyer, P. H.; Hui, C. M.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA. [Christopher, G. E.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P.] NYU, Dept Phys, New York, NY 10003 USA. [DeYoung, T.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Dingus, B. L.; Hoffman, C. M.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Grp P 23, Los Alamos, NM 87545 USA. [Ellsworth, R. W.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [McEnery, J. E.; Vasileiou, V.] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Morgan, T.; Ryan, J. M.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Shoup, A.] Ohio State Univ, Dept Phys, Lima, OH 45804 USA. [Vasileiou, V.] Univ Maryland, Baltimore, MD 21250 USA. RP Abdo, AA (reprint author), USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. EM ebonamen@mtu.edu; petra@mtu.edu RI Saz Parkinson, Pablo Miguel/I-7980-2013; OI Dingus, Brenda/0000-0001-8451-7450; Mincer, Allen/0000-0002-6307-1418 FU National Science Foundation [PHY-0245234, PHY-0302000, PHY-0400424, PHY-0504201, PHY-0601080, PHY-1002445, ATM-0002744]; US Department of Energy (Office of High-Energy Physics and Office of Nuclear Physics); Los Alamos National Laboratory; University of California; Institute of Geophysics and Planetary Physics FX We gratefully acknowledge Scott Delay and Michael Schneider for their dedicated efforts in the construction and maintenance of the Milagro experiment. This work has been supported by the National Science Foundation (under grants PHY-0245234, -0302000, -0400424, -0504201, -0601080, -1002445, and ATM-0002744), the US Department of Energy (Office of High-Energy Physics and Office of Nuclear Physics), the Los Alamos National Laboratory, the University of California, and the Institute of Geophysics and Planetary Physics. NR 23 TC 28 Z9 28 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 JUL 10 PY 2012 VL 753 IS 2 AR 159 DI 10.1088/0004-637X/753/2/159 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700066 ER PT J AU Bell, EF van der Wel, A Papovich, C Kocevski, D Lotz, J McIntosh, DH Kartaltepe, J Faber, SM Ferguson, H Koekemoer, A Grogin, N Wuyts, S Cheung, E Conselice, CJ Dekel, A Dunlop, JS Giavalisco, M Herrington, J Koo, DC McGrath, EJ de Mello, D Rix, HW Robaina, AR Williams, CC AF Bell, Eric F. van der Wel, Arjen Papovich, Casey Kocevski, Dale Lotz, Jennifer McIntosh, Daniel H. Kartaltepe, Jeyhan Faber, S. M. Ferguson, Harry Koekemoer, Anton Grogin, Norman Wuyts, Stijn Cheung, Edmond Conselice, Christopher J. Dekel, Avishai Dunlop, James S. Giavalisco, Mauro Herrington, Jessica Koo, David C. McGrath, Elizabeth J. de Mello, Duilia Rix, Hans-Walter Robaina, Aday R. Williams, Christina C. TI WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z similar to 2 FROM CANDELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: general; galaxies: structure ID DIGITAL SKY SURVEY; MEDIUM-BAND SURVEY; EXTRAGALACTIC LEGACY SURVEY; COSMIC EVOLUTION SURVEY; ACTIVE GALACTIC NUCLEI; K-SELECTED GALAXIES; DEEP FIELD-SOUTH; MASSIVE GALAXIES; STELLAR MASS; ELLIPTIC GALAXIES AB We use HST/WFC3 imaging from the CANDELS Multi-Cycle Treasury Survey, in conjunction with the Sloan Digital Sky Survey, to explore the evolution of galactic structure structure for galaxies with stellar masses >3 x 10(10) M-circle dot from z = 2.2 to the present epoch, a time span of 10 Gyr. We explore the relationship between rest-frame optical color, stellar mass, star formation activity, and galaxy structure. We confirm the dramatic increase from z = 2.2 to the present day in the number density of non-star-forming galaxies above 3 x 10(10) M-circle dot reported by others. We further find that the vast majority of these quiescent systems have concentrated light profiles, as parameterized by the Sersic index, and the population of concentrated galaxies grows similarly rapidly. We examine the joint distribution of star formation activity, Sersic index, stellar mass, inferred velocity dispersion, and stellar surface density. Quiescence correlates poorly with stellar mass at all z < 2.2. Quiescence correlates well with Sersic index at all redshifts. Quiescence correlates well with "velocity dispersion" and stellar surface density at z > 1.3, and somewhat less well at lower redshifts. Yet, there is significant scatter between quiescence and galaxy structure: while the vast majority of quiescent galaxies have prominent bulges, many of them have significant disks, and a number of bulge-dominated galaxies have significant star formation. Noting the rarity of quiescent galaxies without prominent bulges, we argue that a prominent bulge (and perhaps, by association, a supermassive black hole) is an important condition for quenching star formation on galactic scales over the last 10 Gyr, in qualitative agreement with the active galactic nucleus feedback paradigm. C1 [Bell, Eric F.; Herrington, Jessica] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [van der Wel, Arjen; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Papovich, Casey] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Papovich, Casey] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Kocevski, Dale; Faber, S. M.; Cheung, Edmond; Koo, David C.; McGrath, Elizabeth J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Lotz, Jennifer; Ferguson, Harry; Koekemoer, Anton; Grogin, Norman] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McIntosh, Daniel H.] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA. [Kartaltepe, Jeyhan] NOAO Tucson, Tucson, AZ 85719 USA. [Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Dunlop, James S.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Giavalisco, Mauro; Williams, Christina C.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [de Mello, Duilia] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [de Mello, Duilia] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Robaina, Aday R.] IEEC, Inst Ciencies Cosmos, ICC UB, Barcelona 08028, Spain. RP Bell, EF (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ericbell@umich.edu RI Conselice, Christopher/B-4348-2013; OI Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873 FU HST [GO-12060]; NASA through Space Telescope Science Institute [GO-12060]; NASA [NAS5-26555]; Alfred P. Sloan Foundation; National Aeronautics and Space Administration; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; University of Chicago; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Max Planck Institut fur Astronomie; Max Planck Institut fur Astrophysik; New Mexico State University; Princeton University; United States Naval Observatory; University of Washington FX We appreciate the constructive and helpful report from the referee, Pieter van Dokkum. This work is supported by the HST grant GO-12060. Support for Program number GO-12060 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under the NASA contract NAS5-26555.; This publication makes use of the Sloan Digital Sky Survey (SDSS). Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. The SDSS Participating Institutions are the University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Max Planck Institut fur Astronomie, the Max Planck Institut fur Astrophysik, New Mexico State University, Princeton University, the United States Naval Observatory, and the University of Washington. This publication 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/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication also made use of NASA's Astrophysics Data System Bibliographic Services. NR 152 TC 119 Z9 120 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 JUL 10 PY 2012 VL 753 IS 2 AR 167 DI 10.1088/0004-637X/753/2/167 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700074 ER PT J AU Boersma, C Rubin, RH Allamandola, LJ AF Boersma, C. Rubin, R. H. Allamandola, L. J. TI SPATIAL ANALYSIS OF THE POLYCYCLIC AROMATIC HYDROCARBON FEATURES SOUTHEAST OF THE ORION BAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: individual objects (Orion Bar); ISM: lines and bands; molecular data; techniques: spectroscopic ID SPITZER-SPACE-TELESCOPE; INFRARED-EMISSION BANDS; M PAH EMISSION; MU-M; PHOTODISSOCIATION REGION; REFLECTION NEBULAE; IONIZATION FRONT; BENDING MODES; MICRON REGION; SPECTRA AB Polycyclic aromatic hydrocarbon (PAH) and dust emission features between 10 and 37 mu m, observed with Spitzer at 11 positions southeast of the Bright Bar (BB) in Orion, are analyzed and connected to atomic and H-2 lines reported earlier. Variations at these positions indicate changes in local conditions and materials sampled. The major findings are: (1) PAH erosion and destruction are important from the BB out to about 5'. (2) The ionized PAH fraction, inferred from the 11.0 mu m PAH band, increases from the BB out to 6.'5. This counterintuitive behavior is linked to PAH dehydrogenation. (3) The "11.2" mu m PAH band profile shifts from class Lambda(11.2) to Lambda(B)(11.2) between 9' and 10', indicating these lines-of-sight probe a different environment, likely shielded molecular cloud material. (4) The different spatial behavior of the PAH bands and the 10-15 mu m plateau supports the view that the plateau originates in a separate carrier. (5) The fullerene/PAH band strength ratio decreases out to about 7', increases between 9' and 10' and drops at 12'. The first region is where PAHs are dehydrogenated and eroded whereas the second, shielded zone, is where the "11.2" mu m profile shifts and PAH erosion is unlikely. This suggests fullerenes are intimately mixed with PAHs in shielded regions. Taken together, the observations suggest three different regimes are sampled: (1) the H II region-photodissociation region (PDR) interface directly southeast of the BB, (2) shielded molecular cloud material farther out, and (3) the H II region-PDR interface seen limb brightened at the outermost position. C1 [Boersma, C.; Rubin, R. H.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rubin, R. H.] Orion Enterprises, 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 Long Term Space Astrophysics, Astrobiology, Laboratory Astrophysics, NASA's Astronomy + Physics Research and Analysis (APRA) [NNX07AH02G]; NASA Spitzer Space Telescope Support Programs [50082]; NASA 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. Acknowledgements go to an anonymous referee for an exceptionally thorough review and many thoughtful suggestions that have improved the paper. This work was supported through NASA's Long Term Space Astrophysics, Astrobiology, Laboratory Astrophysics, NASA's Astronomy + Physics Research and Analysis (APRA; NNX07AH02G), NASA Spitzer Space Telescope Support Programs (50082), and by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 48 TC 19 Z9 19 U1 1 U2 12 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 JUL 10 PY 2012 VL 753 IS 2 AR 168 DI 10.1088/0004-637X/753/2/168 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700075 ER PT J AU Bond, NA Gawiser, E Guaita, L Padilla, N Gronwall, C Ciardullo, R Lai, K AF Bond, Nicholas A. Gawiser, Eric Guaita, Lucia Padilla, Nelson Gronwall, Caryl Ciardullo, Robin Lai, Kamson TI EVOLUTION IN THE CONTINUUM MORPHOLOGICAL PROPERTIES OF Ly alpha-EMITTING GALAXIES FROM z=3.1 TO z=2.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: formation; galaxies: high-redshift; galaxies: structure ID HUBBLE-DEEP-FIELD; EMISSION-LINE GALAXIES; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; SIMILAR-TO 3; STELLAR POPULATIONS; SOUTH SURVEY; KECK SPECTROSCOPY; SOURCE CATALOGS AB We present a rest-frame ultraviolet morphological analysis of 108 z similar or equal to 2.1 Ly alpha emitters (LAEs) in the Extended Chandra Deep Field South and compare it to a similar sample of 171 LAEs at z similar or equal to 3.1. Using Hubble Space Telescope images from the Galaxy Evolution from Morphology and SEDs survey, Great Observatories Origins Deep Survey, and Hubble Ultradeep Field, we measure size and photometric component distributions, where photometric components are defined as distinct clumps of UV-continuum emission. At both redshifts, >80% of LAEs have observed half-light radii < 2 kpc, but the median half-light radius rises from 0.95 +/- 0.04 kpc at z = 3.1 to 1.41 +/- 0.14 kpc at z = 2.1. A similar evolution is seen in the sizes of individual rest-UV components, but there is no evidence for evolution in the number of multi-component systems. In the z = 2.1 sample, we see clear correlations between the size of an LAE and other physical properties derived from its spectral energy distribution (SED). LAEs are found to be larger for galaxies with higher stellar mass, star formation rate, and dust obscuration, but there is no evidence for a trend between equivalent width and half-light radius at either redshift. The presence of these correlations suggests that a wide range of objects are being selected by LAE surveys at z similar or equal to 2, including a significant fraction of objects for which a massive and moderately extended population of old stars underlies the young starburst giving rise to the Ly alpha emission. C1 [Bond, Nicholas A.; Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Guaita, Lucia] Stockholm Univ, AlbaNova Sci Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Padilla, Nelson] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Gronwall, Caryl; Ciardullo, Robin] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Lai, Kamson] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Bond, Nicholas A.] NASA, Goddard Space Flight Ctr, Cosmol Lab Code 665, Greenbelt, MD 20771 USA. [Padilla, Nelson] Pontificia Univ Catolica Chile, Ctr Astroingn, Santiago, Chile. [Ciardullo, Robin] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. RP Bond, NA (reprint author), Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. FU Eberly College of Science; Office of the Senior Vice President for Research at the Pennsylvania State University; NASA through Space Telescope Science Institute [HST-AR-11253.01-A]; NASA, JPL/Caltech [NAS 5-26555]; National Science Foundation [AST-0807570, AST-0807885]; Department of Energy [DE-FG02-08ER41560, DE-FG02-08ER41561] FX The Institute for Gravitation and the Cosmos is supported by the Eberly College of Science and the Office of the Senior Vice President for Research at the Pennsylvania State University.; This material is based on work supported by NASA through grant number HST-AR-11253.01-A from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555, an award issued by JPL/Caltech, by the National Science Foundation under grants AST-0807570 and AST-0807885, and by the Department of Energy under grants DE-FG02-08ER41560 and DE-FG02-08ER41561. We thank Martin Altmann for the use of his sample of stars in the MUSYC/ECDF-S field. We also thank the referee for helpful comment which improved the clarity of the paper. NR 58 TC 15 Z9 15 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2012 VL 753 IS 2 AR 95 DI 10.1088/0004-637X/753/2/95 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700002 ER PT J AU Brodwin, M Gonzalez, AH Stanford, SA Plagge, T Marrone, DP Carlstrom, JE Dey, A Eisenhardt, PR Fedeli, C Gettings, D Jannuzi, BT Joy, M Leitch, EM Mancone, C Snyder, GF Stern, D Zeimann, G AF Brodwin, M. Gonzalez, A. H. Stanford, S. A. Plagge, T. Marrone, D. P. Carlstrom, J. E. Dey, A. Eisenhardt, P. R. Fedeli, C. Gettings, D. Jannuzi, B. T. Joy, M. Leitch, E. M. Mancone, C. Snyder, G. F. Stern, D. Zeimann, G. TI IDCS J1426.5+3508: SUNYAEV-ZEL'DOVICH MEASUREMENT OF A MASSIVE INFRARED-SELECTED CLUSTER AT z=1.75 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: individual (IDCS J1426.5+3508); galaxies: clusters: intracluster medium; galaxies: evolution ID SOUTH-POLE TELESCOPE; LUMINOUS GALAXY CLUSTER; IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY; GREATER-THAN 1; COSMOLOGY; SAMPLE; EVOLUTION; DISCOVERY; ARRAY AB We report 31 GHz CARMA observations of IDCS J1426.5+3508, an infrared-selected galaxy cluster at z = 1.75. A Sunyaev-Zel'dovich (SZ) decrement is detected toward this cluster, indicating a total mass of M-200,M-m = (4.3 +/- 1.1) x 10(14) M-circle dot in agreement with the approximate X-ray mass of similar to 5 x 10(14) M-circle dot. IDCS J1426.5+3508 is by far the most distant cluster yet detected via the SZ effect, and the most massive z >= 1.4 galaxy cluster found to date. Despite the mere similar to 1% probability of finding it in the 8.82 deg(2) IRAC Distant Cluster Survey, IDCS J1426.5+3508 is not completely unexpected in Lambda CDM once the area of large, existing surveys is considered. IDCS J1426.5+3508 is, however, among the rarest, most extreme clusters ever discovered and indeed is an evolutionary precursor to the most massive known clusters at all redshifts. We discuss how imminent, highly sensitive SZ experiments will complement infrared techniques for statistical studies of the formation of the most massive galaxy clusters in the z > 1.5 universe, including potential precursors to IDCS J1426.5+3508. C1 [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Brodwin, M.; Snyder, G. F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Gonzalez, A. H.; Fedeli, C.; Gettings, D.; Mancone, C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Stanford, S. A.; Zeimann, G.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Plagge, T.; Carlstrom, J. E.; Leitch, E. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Plagge, T.; Carlstrom, J. E.; Leitch, E. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. [Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Eisenhardt, P. R.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Joy, M.] NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Brodwin, M (reprint author), Univ Missouri, Dept Phys & Astron, 5110 Rockhill Rd, Kansas City, MO 64110 USA. OI Marrone, Daniel/0000-0002-2367-1080 FU National Science Foundation [AST-0838187, PHY-0114422]; CARMA; NASA; NASA by JPL/Caltech; Smithsonian Astrophysical Observatory; NASA [G09-0150A, NAS 5-26555]; NASA through Space Telescope Science Institute [11663, 12203]; W. M. Keck Foundation; U.S. Department of Energy [W-7405-ENG-48]; CARMA construction; [SV4-74018, A31] 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, and by the CARMA partner universities. The work at Chicago is supported by NSF grants AST-0838187 and PHY-0114422.; 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. This work is based in part on observations obtained with the Chandra X-Ray Observatory (Chandra), under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory, which operates Chandra for NASA. Support for this research was provided by the NASA grant G09-0150A. Support for HST programs 11663 and 12203 were provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under the NASA contract NAS 5-26555. This work is based in part on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work makes use of image data from the NOAO DeepWide-Field Survey (NDWFS) as distributed by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation.; We thank the anonymous referee for suggestions that improved the manuscript, Bradford Benson for helpful discussions, F. Will High and Keith Vanderlinde for providing published SPT masses in a digital form, Matt Ashby for creating the IRAC catalogs for SDWFS, Michael Brown for combining the NDWFS with SDWFS catalogs, Alexey Vikhlinin for advice on the analysis of the Chandra data, and Daniel Holz for providing his predictions in an electronic format. This paper would not have been possible without the efforts of the support staffs of CARMA, the Keck Observatory, the Spitzer Space Telescope, the Hubble Space Telescope, and the Chandra X-Ray Observatory. Support for M.B. was provided by the W. M. Keck Foundation. A.H.G. acknowledges support from the National Science Foundation performed under the auspices of the U.S. Department of Energy under Contract No. W-7405-ENG-48. NR 59 TC 39 Z9 39 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 JUL 10 PY 2012 VL 753 IS 2 AR 162 DI 10.1088/0004-637X/753/2/162 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700069 ER PT J AU Dheeraj, PR Strohmayer, TE AF Dheeraj, Pasham R. Strohmayer, Tod E. TI A MULTI-EPOCH TIMING AND SPECTRAL STUDY OF THE ULTRALUMINOUS X-RAY NGC 5408 X-1 WITH XMM-Newton SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; methods: observational; X-rays: binaries ID QUASI-PERIODIC OSCILLATIONS; MASS BLACK-HOLES; MICROQUASAR GRO J1655-40; HIGH-RESOLUTION CAMERA; XTE J1550-564; VARIABILITY; DISCOVERY; FREQUENCY; M82; ACCRETION AB We present results of new XMM-Newton observations of the ultraluminous X-ray source (ULX) NGC 5408 X-1, one of the few ULXs to show quasi-periodic oscillations (QPOs). We detect QPOs in each of four new (approximate to 100 ks) pointings, expanding the range of frequencies observed from 10 to 40 mHz. We compare our results with the timing and spectral correlations seen in stellar-mass black hole systems, and find that the qualitative nature of the timing and spectral behavior of NGC 5408 X-1 is similar to systems in the steep power-law state exhibiting Type-C QPOs. However, in order for this analogy to quantitatively hold we must only be seeing the so-called saturated portion of the QPO frequency-photon index (or disk flux) relation. Assuming this to be the case, we place a lower limit on the mass of NGC 5408 X-1 of greater than or similar to 800 M-circle dot. Alternatively, the QPO frequency is largely independent of the spectral parameters, in which case a close analogy with the Type-C QPOs in stellar systems is problematic. Measurement of the source's timing properties over a wider range of energy spectral index is needed to definitively resolve this ambiguity. We searched all the available data for both a broad Fe emission line as well as high-frequency QPO analogs (0.1-1 Hz), but detected neither. We place upper limits on the equivalent width of any Fe emission feature in the 6-7 keV band and of the amplitude (rms) of a high-frequency QPO analog of approximate to 10 eV and approximate to 4%, respectively. C1 [Dheeraj, Pasham R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Strohmayer, Tod E.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Dheeraj, PR (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM dheeraj@astro.umd.edu; tod.strohmayer@nasa.gov NR 52 TC 12 Z9 12 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2012 VL 753 IS 2 AR 139 DI 10.1088/0004-637X/753/2/139 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700046 ER PT J AU Donaldson, JK Roberge, A Chen, CH Augereau, JC Dent, WRF Eiroa, C Krivov, AV Mathews, GS Meeus, G Menard, F Riviere-Marichalar, P Sandell, G AF Donaldson, J. K. Roberge, A. Chen, C. H. Augereau, J. -C. Dent, W. R. F. Eiroa, C. Krivov, A. V. Mathews, G. S. Meeus, G. Menard, F. Riviere-Marichalar, P. Sandell, G. TI HERSCHEL PACS OBSERVATIONS AND MODELING OF DEBRIS DISKS IN THE TUCANA-HOROLOGIUM ASSOCIATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars ID SPITZER-SPACE-TELESCOPE; SOLAR-TYPE STARS; T-TAURI STARS; PLANETARY-SYSTEMS; SIZE DISTRIBUTIONS; BETA-PICTORIS; INFRARED SPECTROGRAPH; DUST DYNAMICS; NEARBY STARS; KUIPER-BELT AB We present Herschel PACS photometry of 17 B- to M-type stars in the 30 Myr old Tucana-Horologium Association. This work is part of the Herschel Open Time Key Programme "Gas in Protoplanetary Systems". 6 of the 17 targets were found to have infrared excesses significantly greater than the expected stellar IR fluxes, including a previously unknown disk around HD30051. These six debris disks were fitted with single-temperature blackbody models to estimate the temperatures and abundances of the dust in the systems. For the five stars that show excess emission in the Herschel PACS photometry and also have Spitzer IRS spectra, we fit the data with models of optically thin debris disks with realistic grain properties in order to better estimate the disk parameters. The model is determined by a set of six parameters: surface density index, grain size distribution index, minimum and maximum grain sizes, and the inner and outer radii of the disk. The best-fitting parameters give us constraints on the geometry of the dust in these systems, as well as lower limits to the total dust masses. The HD105 disk was further constrained by fitting marginally resolved PACS 70 mu m imaging. C1 [Donaldson, J. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Roberge, A.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chen, C. H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Augereau, J. -C.; Menard, F.] UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, F-38041 Grenoble, France. [Dent, W. R. F.] ALMA, Santiago, Chile. [Dent, W. R. F.] European So Observ, Santiago 19, Chile. [Eiroa, C.; Meeus, G.] Univ Autonoma Madrid, Fac Ciencias, Dpt Fis Teor, E-28049 Madrid, Spain. [Krivov, A. V.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany. [Mathews, G. S.] Univ Hawaii, Inst Astron IfA, Honolulu, HI 96822 USA. [Riviere-Marichalar, P.] Ctr Astrobiol Depto Astrofis CSIC INTA, Villanueva De La Canada 28691, Spain. [Sandell, G.] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Donaldson, JK (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM jessd@astro.umd.edu RI Roberge, Aki/D-2782-2012 OI Roberge, Aki/0000-0002-2989-3725 FU NASA through JPL/Caltech; PNP-CNES; French National Research Agency (ANR) [ANR-2010 BLAN-0505-01 (EXOZODI)] FX This work is based on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. J.C.A. thanks the PNP-CNES and the French National Research Agency (ANR) for financial support through contract ANR-2010 BLAN-0505-01 (EXOZODI). NR 65 TC 18 Z9 18 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2012 VL 753 IS 2 AR 147 DI 10.1088/0004-637X/753/2/147 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700054 ER PT J AU Gonzalez, AH Stanford, SA Brodwin, M Fedeli, C Dey, A Eisenhardt, PRM Mancone, C Stern, D Zeimann, G AF Gonzalez, Anthony H. Stanford, S. Adam Brodwin, Mark Fedeli, Cosimo Dey, Arjun Eisenhardt, Peter R. M. Mancone, Conor Stern, Daniel Zeimann, Greg TI IDCS J1426.5+3508: COSMOLOGICAL IMPLICATIONS OF A MASSIVE, STRONG LENSING CLUSTER AT z=1.75 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; cosmology: observations; galaxies: clusters: individual (IDCS J1426.5+3508); gravitational lensing: strong ID GIANT-ARC STATISTICS; DARK-MATTER HALOES; GALAXY CLUSTERS; CROSS-SECTIONS; UNIVERSE; FIELD; POPULATION; POTENTIALS; SIMULATION; DEPENDENCE AB The galaxy cluster IDCS J1426.5+3508 at z = 1.75 is the most massive galaxy cluster yet discovered at z > 1.4 and the first cluster at this epoch for which the Sunyaev-Zel'Dovich effect has been observed. In this paper, we report on the discovery with Hubble Space Telescope imaging of a giant arc associated with this cluster. The curvature of the arc suggests that the lensing mass is nearly coincident with the brightest cluster galaxy, and the color is consistent with the arc being a star-forming galaxy. We compare the constraint on M-200 based upon strong lensing with Sunyaev-Zel'Dovich results, finding that the two are consistent if the redshift of the arc is z greater than or similar to 3. Finally, we explore the cosmological implications of this system, considering the likelihood of the existence of a strongly lensing galaxy cluster at this epoch in a Lambda CDM universe. While the existence of the cluster itself can potentially be accommodated if one considers the entire volume covered at this redshift by all current high-redshift cluster surveys, the existence of this strongly lensed galaxy greatly exacerbates the long-standing giant arc problem. For standard Lambda CDM structure formation and observed background field galaxy counts this lens system should not exist. Specifically, there should be no giant arcs in the entire sky as bright in F814W as the observed arc for clusters at z >= 1.75, and only similar to 0.3 as bright in F160W as the observed arc. If we relax the redshift constraint to consider all clusters at z >= 1.5, the expected number of giant arcs rises to similar to 15 in F160W, but the number of giant arcs of this brightness in F814W remains zero. These arc statistic results are independent of the mass of IDCS J1426.5+3508. We consider possible explanations for this discrepancy. C1 [Gonzalez, Anthony H.; Fedeli, Cosimo; Mancone, Conor] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Stanford, S. Adam; Zeimann, Greg] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. Adam] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Brodwin, Mark] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA. [Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Eisenhardt, Peter R. M.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gonzalez, AH (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. FU Nancy Levenson; NASA through HST GO programs [11663, 12203]; National Science Foundation [AST-0708490]; U.S. Department of Energy [W-7405-ENG-48]; NOAO; NASA FX The authors thank the anonymous referee for suggestions that improved the quality of this paper. We are also grateful to the Gemini Observatory for allocating Director's Discretionary time to obtain a redshift for the giant arc. We appreciate the support provided by Nancy Levenson and the rest of the Gemini staff for this project. Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). This work is based in part on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. Support for this research was provided by NASA through HST GO programs 11663 and 12203. A.H.G. thanks Marusa Bradac for a useful discussion about the arc, and also acknowledges support from the National Science Foundation through the grant AST-0708490. The work by S.A.S. at LLNL was performed under the auspices of the U.S. Department of Energy under Contract No. W-7405-ENG-48, and support for M.B. was provided by the W. M. Keck Foundation. The work of P.R.M.E. and D.S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The research activities of A.D. are supported by NOAO, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. NR 58 TC 22 Z9 22 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2012 VL 753 IS 2 AR 163 DI 10.1088/0004-637X/753/2/163 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700070 ER PT J AU Kirkpatrick, JD Gelino, CR Cushing, MC Mace, GN Griffith, RL Skrutskie, MF Marsh, KA Wright, EL Eisenhardt, PR McLean, IS Mainzer, AK Burgasser, AJ Tinney, CG Parker, S Salter, G AF Kirkpatrick, J. Davy Gelino, Christopher R. Cushing, Michael C. Mace, Gregory N. Griffith, Roger L. Skrutskie, Michael F. Marsh, Kenneth A. Wright, Edward L. Eisenhardt, Peter R. McLean, Ian S. Mainzer, Amanda K. Burgasser, Adam J. Tinney, C. G. Parker, Stephen Salter, Graeme TI FURTHER DEFINING SPECTRAL TYPE "Y" AND EXPLORING THE LOW-MASS END OF THE FIELD BROWN DWARF MASS FUNCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; solar neighborhood; stars: low-mass; stars: luminosity function, mass function; surveys; techniques: spectroscopic ID ALL-SKY SURVEY; PROPER-MOTION STARS; INFRARED-SURVEY-EXPLORER; LARGE-AREA SURVEY; SURVEY COMMISSIONING DATA; MULTIPLE SYSTEM LHS-1070; EXTRASOLAR GIANT PLANETS; SPITZER-SPACE-TELESCOPE; KECK II TELESCOPE; XI URSAE-MAJORIS AB We present the discovery of another seven Y dwarfs from the Wide-field Infrared Survey Explorer (WISE). Using these objects, as well as the first six WISE Y dwarf discoveries from Cushing et al., we further explore the transition between spectral types T and Y. We find that the T/Y boundary roughly coincides with the spot where the J-H colors of brown dwarfs, as predicted by models, turn back to the red. Moreover, we use preliminary trigonometric parallax measurements to show that the T/Y boundary may also correspond to the point at which the absolute H (1.6 mu m) and W2 (4.6 mu m) magnitudes plummet. We use these discoveries and their preliminary distances to place them in the larger context of the solar neighborhood. We present a table that updates the entire stellar and substellar constituency within 8 pc of the Sun, and we show that the current census has hydrogen-burning stars outnumbering brown dwarfs by roughly a factor of six. This factor will decrease with time as more brown dwarfs are identified within this volume, but unless there is a vast reservoir of cold brown dwarfs invisible to WISE, the final space density of brown dwarfs is still expected to fall well below that of stars. We also use these new Y dwarf discoveries, along with newly discovered T dwarfs from WISE, to investigate the field substellar mass function. We find that the overall space density of late-T and early-Y dwarfs matches that from simulations describing the mass function as a power law with slope -0.5 < alpha < 0.0; however, a power law may provide a poor fit to the observed object counts as a function of spectral type because there are tantalizing hints that the number of brown dwarfs continues to rise from late-T to early-Y. More detailed monitoring and characterization of these Y dwarfs, along with dedicated searches aimed at identifying more examples, are certainly required. C1 [Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Marsh, Kenneth A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Mace, Gregory N.; Wright, Edward L.; McLean, Ian S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Eisenhardt, Peter R.; Mainzer, Amanda K.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Burgasser, Adam J.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Tinney, C. G.; Parker, Stephen; Salter, Graeme] Univ New S Wales, Dept Astrophys, Sch Phys, Sydney, NSW 2052, Australia. RP Kirkpatrick, JD (reprint author), CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA. EM davy@ipac.caltech.edu OI Tinney, Christopher/0000-0002-7595-0970 FU National Aeronautics and Space Administration; National Science Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; U.S. Government [NAGW-2166]; NASA by JPL/Caltech [70062, 80109]; NASA [NAS 5-26555]; NASA through the Space Telescope Science Institute; W. M. Keck Foundation FX We thank the referee, Sandy Leggett, for constructive comments that helped to improve the paper. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from 2MASS, SDSS, and DSS. 2MASS 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. SDSS is funded 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 DSS were produced at the Space Telescope Science Institute under U.S. Government grant NAGW-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope.; 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 to program 70062 and 80109 by JPL/Caltech. This work is also based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, 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 12044 and 12330. Support for these programs was provided by NASA through a grant from the Space Telescope Science Institute. Some of the spectroscopic 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. In acknowledgement of our observing time at Keck and the IRTF, we further wish to recognize the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 225 TC 122 Z9 122 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2012 VL 753 IS 2 AR 156 DI 10.1088/0004-637X/753/2/156 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700063 ER PT J AU Kogut, A AF Kogut, A. TI SYNCHROTRON SPECTRAL CURVATURE FROM 22 MHz TO 23 GHz SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiation mechanisms: non-thermal; radio continuum: general ID 45-MHZ CONTINUUM SURVEY; PROBE WMAP OBSERVATIONS; SPINNING DUST GRAINS; FOREGROUND EMISSION; MICROWAVE EMISSION; GALACTIC EMISSION; RADIO-EMISSION; SKY MAPS; RADIATION; POLARIZATION AB We combine surveys of the radio sky at frequencies 22 MHz to 1.4 GHz with data from the ARCADE-2 instrument at frequencies 3 GHz to 10 GHz to characterize the frequency spectrum of diffuse synchrotron emission in the Galaxy. The radio spectrum steepens with frequency from 22 MHz to 10 GHz. The projected spectral index at 23 GHz derived from the low-frequency data agrees well with independent measurements using only data at frequencies 23 GHz and above. Comparing the spectral index at 23 GHz to the value from previously published analyses allows extension of the model to higher frequencies. The combined data are consistent with a power-law index beta = -2.64 +/- 0.03 at 0.31 GHz, steepening by an amount of Delta beta = 0.07 every octave in frequency. Comparison of the radio data to models including the cosmic-ray energy spectrum suggests that any break in the synchrotron spectrum must occur at frequencies above 23 GHz. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kogut, A (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. EM Alan.J.Kogut@nasa.gov FU National Aeronautics and Space Administration through the Science Mission Directorate FX This research is based upon work supported by the National Aeronautics and Space Administration through the Science Mission Directorate under the Astronomy and Physics Research and Analysis suborbital program. NR 34 TC 13 Z9 13 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 JUL 10 PY 2012 VL 753 IS 2 AR 110 DI 10.1088/0004-637X/753/2/110 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700017 ER PT J AU Kusakabe, N Grady, CA Sitko, ML Hashimoto, J Kudo, T Fukagawa, M Muto, T Wisniewski, JP Min, M Mayama, S Werren, C Day, AN Beerman, LC Lynch, DK Russell, RW Brafford, SM Kuzuhara, M Brandt, TD Abe, L Brandner, W Carson, J Egner, S Feldt, M Goto, M Guyon, O Hayano, Y Hayashi, M Hayashi, SS Henning, T Hodapp, KW Ishii, M Iye, M Janson, M Kandori, R Knapp, GR Matsuo, T McElwain, MW Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Suto, H Suzuki, R Takami, M Takato, N Terada, H Thalmann, C Tomono, D Turner, EL Watanabe, M Yamada, T Takami, H Usuda, T Tamura, M AF Kusakabe, N. Grady, C. A. Sitko, M. L. Hashimoto, J. Kudo, T. Fukagawa, M. Muto, T. Wisniewski, J. P. Min, M. Mayama, S. Werren, C. Day, A. N. Beerman, L. C. Lynch, D. K. Russell, R. W. Brafford, S. M. Kuzuhara, M. Brandt, T. D. Abe, L. Brandner, W. Carson, J. Egner, S. Feldt, M. Goto, M. Guyon, O. Hayano, Y. Hayashi, M. Hayashi, S. S. Henning, T. Hodapp, K. W. Ishii, M. Iye, M. Janson, M. Kandori, R. Knapp, G. R. Matsuo, T. McElwain, M. W. Miyama, S. Morino, J. -I. Moro-Martin, A. Nishimura, T. Pyo, T. -S. Suto, H. Suzuki, R. Takami, M. Takato, N. Terada, H. Thalmann, C. Tomono, D. Turner, E. L. Watanabe, M. Yamada, T. Takami, H. Usuda, T. Tamura, M. TI HIGH-CONTRAST NEAR-INFRARED POLARIZATION IMAGING OF MWC480 SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars: individual (MWC 480); stars: pre-main sequence ID PRE-MAIN-SEQUENCE; HERBIG-AE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; PROTOPLANETARY DISKS; AE/BE STARS; FILTER SET; CIRCUMSTELLAR DUST; TELESCOPE FACILITY; PLANET FORMATION; STANDARD STARS AB One of the key predictions of modeling from the IR excess of Herbig Ae stars is that for protoplanetary disks, where significant grain growth and settling has occurred, the dust disk has flattened to the point that it can be partially or largely shadowed by the innermost material at or near the dust sublimation radius. When the self-shadowing has already started, the outer disk is expected to be detected in scattered light only in the exceptional cases when the scale height of the dust disk at the sublimation radius is smaller than usual. High-contrast imaging combined with the IR spectral energy distribution allow us to measure the degree of flattening of the disk, as well as to determine the properties of the outer disk. We present polarimetric differential imaging in the H band obtained with Subaru/HiCIAO of one such system, MWC 480. The HiCIAO data were obtained at a historic minimum of the NIR excess. The disk is detected in scattered light from 0.'' 2 to 1.'' 0 (27.4-137AU). Together with the marginal detection of the disk from 1998 February 24 by Hubble Space Telescope/NICMOS, our data constrain the opening half-angle for the disk to lie between 1.degrees 3 <= theta <= 2 degrees.2. When compared with similar measures in CO for the gas disk from the literature, the dust disk subtends only similar to 30% of the gas disk scale height (H/R similar to 0.03). Such a dust disk is a factor of 5-7 flatter than transitional disks, which have structural signatures that giant planets have formed. C1 [Kusakabe, N.; Hashimoto, J.; Kudo, T.; Iye, M.; Kandori, R.; Miyama, S.; Morino, J. -I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. [Grady, C. A.] Eureka Sci, Oakland, CA 96402 USA. [Sitko, M. L.; Werren, C.; Day, A. N.; Beerman, L. C.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Sitko, M. L.] Space Sci Inst, Boulder, CO 80301 USA. [Fukagawa, M.] Osaka Univ, Dept Earth & Space Sci, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan. [Muto, T.] Tokyo Inst Technol, Meguro Ku, Tokyo 1528551, Japan. [Muto, T.] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan. [Wisniewski, J. P.] Univ Washington, Dept Astron, Washington, DC USA. [Min, M.; Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Mayama, S.] Grad Univ Adv Studies, Ctr Promot Integrated Sci, Shonan Int Village Hayam, Kanagawa, Japan. [Lynch, D. K.; Russell, R. W.] Aerosp Corp, Los Angeles, CA 90009 USA. [Brafford, S. M.] Brafford & Phillips, Batavia, OH 45103 USA. [Kuzuhara, M.] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Brandt, T. D.; Janson, M.; Knapp, G. R.; Moro-Martin, A.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Abe, L.] Univ Nice Sophia Antipolis, Lab Lagrange, CNRS, Observ Cote Azur,UMR7293, F-06300 Nice, France. [Brandner, W.; Feldt, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S. S.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Subaru Telescope, Hilo, HI 96720 USA. [Goto, M.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany. [Hayashi, M.; Ishii, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [McElwain, M. W.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Moro-Martin, A.] Inst Nacl Tecn Aeroespacial, Dept Astrofis, CAB INTA CSIC, Madrid 28850, Spain. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Turner, E. L.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2278568, Japan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. [Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Kusakabe, N (reprint author), Natl Astron Observ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM nb.kusakabe@nao.ac.jp RI Turner, Edwin/A-4295-2011; MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016 OI Watanabe, Makoto/0000-0002-3656-4081 FU KAKENHI [22000005, 23103004, 23740151]; NSF AST [1008440, 1009314]; NASA [NNX09AC73G]; IR&D program at The Aerospace Corporation FX This work is partially supported by KAKENHI 22000005 (M.T.), KAKENHI 23103004, 23740151 (M.F.), NSF AST 1008440 (C.A.G.), NSF AST 1009314 (J.P.W.), NASA NNX09AC73G (C.A.G. and M.L.S.), and the IR&D program at The Aerospace Corporation (R.W.R.). NR 52 TC 31 Z9 31 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2012 VL 753 IS 2 AR 153 DI 10.1088/0004-637X/753/2/153 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700060 ER PT J AU Stanford, SA Brodwin, M Gonzalez, AH Zeimann, G Stern, D Dey, A Eisenhardt, PR Snyder, GF Mancone, C AF Stanford, S. A. Brodwin, M. Gonzalez, Anthony H. Zeimann, Greg Stern, Daniel Dey, Arjun Eisenhardt, P. R. Snyder, Gregory F. Mancone, C. TI IDCS J1426.5+3508: DISCOVERY OF A MASSIVE, INFRARED-SELECTED GALAXY CLUSTER AT z=1.75 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual; galaxies: distances and redshifts; galaxies: evolution ID IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY; PROBE; DEEP; CONSTRAINTS; EXTRACTION; RESOLUTION; SOFTWARE; XBOOTES; PROFILE AB We report the discovery of an IR-selected massive galaxy cluster in the IRAC Deep Cluster Survey (IDCS). We present new data from the Hubble Space Telescope and the W. M. Keck Observatory that spectroscopically confirm IDCS J1426.5+3508 at z = 1.75. Moreover, the cluster is detected in archival Chandra data as an extended X-ray source, comprising 53 counts after the removal of point sources. We calculate an X-ray luminosity of L0.5-2 keV = (5.4 +/- 1.2) x 10(44) erg s(-1) within r = 60 arcsec (similar to 1 Mpc diameter), which implies M-200,M- Lx = (5.3 +/- 1.6) x 10(14) M-circle dot. IDCS J1426.5+3508 appears to be an exceptionally massive cluster for its redshift. C1 [Stanford, S. A.; Zeimann, Greg] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Stanford, S. A.; Snyder, Gregory F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gonzalez, Anthony H.; Mancone, C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Stern, Daniel; Eisenhardt, P. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Stanford, SA (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. EM stanford@physics.ucdavis.edu FU NASA [G09-0150A, NAS 5-26555]; National Science Foundation [AST-0708490]; NASA by JPL/Caltech; NASA through a grant from the Space Telescope Science Institute [11663, 12203]; W. M. Keck Foundation; U. S. Department of Energy [W-7405-ENG-48]; [SV4-74018, A31] FX This work is based in part on observations obtained with the Chandra X-Ray Observatory (Chandra), under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory which operates Chandra for NASA. Support for this research was provided by the NASA grant G09-0150A. A.H.G. acknowledges support from the National Science Foundation through grant AST-0708490. 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. Support for HST programs 11663 and 12203 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work makes use of image data from the NOAO Deep Wide-Field Survey (NDWFS) as distributed by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation.; We thank Matt Ashby for creating the IRAC catalogs for SDWFS, Buell Jannuzi for his work on the NDWFS, Michael Brown for combining the NDWFS with SDWFS catalogs, Steve Murray and his XBootes team for obtaining the Chandra data in the Bootes field, and Alexey Vihklinin for advice on the analysis of the Chandra data. We also thank the referee for a report which helped to improve the presentation and interpretation of the results. This paper would not have been possible without the efforts of the support staffs of the Keck Observatory, the Spitzer Space Telescope, the Hubble Space Telescope, and the Chandra X-Ray Observatory. Support for M. B. was provided by the W. M. Keck Foundation. The work by S.A.S. at LLNL was performed under the auspices of the U. S. Department of Energy under Contract No. W-7405-ENG-48. NR 47 TC 71 Z9 71 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 JUL 10 PY 2012 VL 753 IS 2 AR 164 DI 10.1088/0004-637X/753/2/164 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700071 ER PT J AU Teng, SH Schawinski, K Urry, CM Darg, DW Kaviraj, S Oh, K Bonning, EW Cardamone, CN Keel, WC Lintott, CJ Simmons, BD Treister, E AF Teng, Stacy H. Schawinski, Kevin Urry, C. Megan Darg, Dan W. Kaviraj, Sugata Oh, Kyuseok Bonning, Erin W. Cardamone, Carolin N. Keel, William C. Lintott, Chris J. Simmons, Brooke D. Treister, Ezequiel TI CHANDRA OBSERVATIONS OF GALAXY ZOO MERGERS: FREQUENCY OF BINARY ACTIVE NUCLEI IN MASSIVE MERGERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; X-rays: galaxies ID SUPERMASSIVE BLACK-HOLES; STAR-FORMATION RATE; DIGITAL-SKY-SURVEY; ULTRALUMINOUS INFRARED GALAXIES; X-RAY; GALACTIC NUCLEUS; HOST GALAXIES; MERGING GALAXIES; NEARBY UNIVERSE; MORPHOLOGIES AB We present the results from a Chandra pilot study of 12 massive galaxy mergers selected from Galaxy Zoo. The sample includes major mergers down to a host galaxy mass of 10(11) M-circle dot that already have optical active galactic nucleus (AGN) signatures in at least one of the progenitors. We find that the coincidences of optically selected active nuclei with mildly obscured (N-H less than or similar to 1.1 x 10(22) cm(-2)) X-ray nuclei are relatively common (8/12), but the detections are too faint (<40 counts per nucleus; f(2-10 keV) less than or similar to 1.2 x 10(-13) erg s(-1) cm(-2)) to reliably separate starburst and nuclear activity as the origin of the X-ray emission. Only one merger is found to have confirmed binary X-ray nuclei, though the X-ray emission from its southern nucleus could be due solely to star formation. Thus, the occurrences of binary AGNs in these mergers are rare (0%-8%), unless most merger-induced active nuclei are very heavily obscured or Compton thick. C1 [Teng, Stacy H.] NASA, Observat Cosmol Lab, GSFC, Greenbelt, MD 20771 USA. [Teng, Stacy H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Schawinski, Kevin; Urry, C. Megan; Bonning, Erin W.] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Schawinski, Kevin; Urry, C. Megan; Bonning, Erin W.; Simmons, Brooke D.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Urry, C. Megan; Simmons, Brooke D.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Darg, Dan W.; Kaviraj, Sugata; Lintott, Chris J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Oh, Kyuseok] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Cardamone, Carolin N.] Brown Univ, Harriet W Sheridan Ctr Teaching & Learning, Providence, RI 02912 USA. [Keel, William C.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Treister, Ezequiel] Univ Concepcion, Dept Astron, Concepcion, Chile. RP Teng, SH (reprint author), NASA, Observat Cosmol Lab, GSFC, Greenbelt, MD 20771 USA. EM stacy.h.teng@nasa.gov RI Urry, Claudia/G-7381-2011; OI Urry, Claudia/0000-0002-0745-9792; Schawinski, Kevin/0000-0001-5464-0888; Simmons, Brooke/0000-0001-5882-3323 FU NASA by the Chandra X-Ray Observatory Center [PF9-00069]; NASA through the Chandra General Observer Program [GO1-121401]; NASA [NAS8-03060] FX We thank the anonymous referee for his or her prompt and careful comments which improved the manuscript. We made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. We acknowledge support by NASA through the Chandra General Observer Program grant GO1-121401 to Yale University. S.H.T. is supported by a NASA Postdoctoral Fellowship and K.S. is supported by NASA through an Einstein Postdoctoral Fellowship Grant No. PF9-00069 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. NR 47 TC 13 Z9 13 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 JUL 10 PY 2012 VL 753 IS 2 AR 165 DI 10.1088/0004-637X/753/2/165 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700072 ER PT J AU Wharton, RS Chatterjee, S Cordes, JM Deneva, JS Lazio, TJW AF Wharton, R. S. Chatterjee, S. Cordes, J. M. Deneva, J. S. Lazio, T. J. W. TI MULTIWAVELENGTH CONSTRAINTS ON PULSAR POPULATIONS IN THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; pulsars: general ID SAGITTARIUS-A-ASTERISK; NUCLEAR STAR CLUSTER; SUPERMASSIVE BLACK-HOLE; LARGE-AREA TELESCOPE; X-RAY-EMISSION; RADIO PULSARS; MILLISECOND PULSARS; GLOBULAR-CLUSTERS; CENTRAL PARSEC; WIND NEBULAE AB The detection of radio pulsars within the central few parsecs of the Galaxy would provide a unique probe of the gravitational and magneto-ionic environments in the Galactic center (GC) and, if close enough to Sgr A*, precise tests of general relativity in the strong-field regime. While it is difficult to find pulsars at radio wavelengths because of interstellar scattering, the payoff from detailed timing of pulsars in the GC warrants a concerted effort. To motivate pulsar surveys and help define search parameters for them, we constrain the pulsar number and spatial distribution using a wide range of multiwavelength measurements. These include the five known radio pulsars within 15' of Sgr A*, non-detections in high-frequency pulsar surveys of the central parsec, radio and gamma-ray measurements of diffuse emission, a catalog of radio point sources from an imaging survey, infrared observations of massive star populations in the central few parsecs, candidate pulsar wind nebulae in the inner 20 pc, and estimates of the core-collapse supernova rate based on X-ray measurements. We find that under current observational constraints, the inner parsec of the Galaxy could harbor as many as similar to 10(3) active radio pulsars that are beamed toward Earth. Such a large population would distort the low-frequency measurements of both the intrinsic spectrum of Sgr A* and the free-free absorption along the line of sight of Sgr A*. C1 [Wharton, R. S.; Chatterjee, S.; Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Deneva, J. S.] Arecibo Observ, Arecibo, PR 00612 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wharton, RS (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM rwharton@astro.cornell.edu FU Cornell University by NSF [AST-1008213, AST-1109411] FX We thank the anonymous referee for helpful comments that improved the clarity of this paper. This research was supported at Cornell University by NSF grants AST-1008213 and AST-1109411. Part of this research was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics & Space Administration. We have also made use of NASA's Astrophysics Data System. NR 76 TC 38 Z9 38 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 JUL 10 PY 2012 VL 753 IS 2 AR 108 DI 10.1088/0004-637X/753/2/108 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967MR UT WOS:000305912700015 ER PT J AU Abdo, AA Abeysekara, AU Allen, BT Aune, T Berley, D Chen, C Christopher, GE DeYoung, T Dingus, BL Ellsworth, RW Gonzalez, MM Goodman, JA Granot, J Hays, E Hoffman, CM Huntemeyer, PH Kolterman, BE Linnemann, JT McEnery, JE Mincer, AI Morgan, T Nemethy, P Pretz, J Ramirez-Ruiz, E Ryan, JM Parkinson, PMS Shoup, A Sinnis, G Smith, AJ Vasileiou, V Walker, GP Williams, DA Yodh, GB AF Abdo, A. A. Abeysekara, A. U. Allen, B. T. Aune, T. Berley, D. Chen, C. Christopher, G. E. DeYoung, T. Dingus, B. L. Ellsworth, R. W. Gonzalez, M. M. Goodman, J. A. Granot, J. Hays, E. Hoffman, C. M. Huentemeyer, P. H. Kolterman, B. E. Linnemann, J. T. McEnery, J. E. Mincer, A. I. Morgan, T. Nemethy, P. Pretz, J. Ramirez-Ruiz, E. Ryan, J. M. Parkinson, P. M. Saz Shoup, A. Sinnis, G. Smith, A. J. Vasileiou, V. Walker, G. P. Williams, D. A. Yodh, G. B. TI CONSTRAINTS ON THE EMISSION MODEL OF THE "NAKED-EYE BURST" GRB 080319B SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astroparticle physics; gamma-ray burst: individual (GRB 080319B) ID HIGH-ENERGY EMISSION; GAMMA-RAY BURSTS; FERMI OBSERVATIONS; PROMPT; SHOCKS AB On 2008 March 19, one of the brightest gamma-ray bursts (GRBs) ever recorded was detected by several ground- and space-based instruments spanning the electromagnetic spectrum from radio to gamma rays. With a peak visual magnitude of 5.3, GRB 080319B was dubbed the "naked-eye" GRB, as an observer under dark skies could have seen the burst without the aid of an instrument. Presented here are results from observations of the prompt phase of GRB 080319B taken with the Milagro TeV observatory. The burst was observed at an elevation angle of 47 degrees. Analysis of the data is performed using both the standard air shower method and the scaler or single-particle technique, which results in a sensitive energy range that extends from similar to 5 GeV to >20 TeV. These observations provide the only direct constraints on the properties of the high-energy gamma-ray emission from GRB 080319B at these energies. No evidence for emission is found in the Milagro data, and upper limits on the gamma-ray flux above 10 GeV are derived. The limits on emission between similar to 25 and 200 GeV are incompatible with the synchrotron self-Compton model of gamma-ray production and disfavor a corresponding range (2 eV-16 eV) of assumed synchrotron peak energies. This indicates that the optical photons and soft (similar to 650 keV) gamma rays may not be produced by the same electron population. C1 [Aune, T.; Parkinson, P. M. Saz; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Abdo, A. A.; Abeysekara, A. U.; Linnemann, J. T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Abdo, A. A.; Ellsworth, R. W.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Allen, B. T.; Chen, C.; Yodh, G. B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Berley, D.; Goodman, J. A.; Smith, A. J.; Vasileiou, V.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Christopher, G. E.; Kolterman, B. E.; Mincer, A. I.; Pretz, J.] NYU, Dept Phys, New York, NY 10003 USA. [DeYoung, T.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Dingus, B. L.; Hoffman, C. M.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Grp P 23, Los Alamos, NM 87545 USA. [Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Granot, J.] Open Univ Israel, IL-43537 Raanana, Israel. [Hays, E.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huentemeyer, P. H.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA. [Morgan, T.; Ryan, J. M.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Shoup, A.] Ohio State Univ, Dept Phys, Lima, OH 45804 USA. RP Aune, T (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, 1156 High St, Santa Cruz, CA 95064 USA. RI Saz Parkinson, Pablo Miguel/I-7980-2013; Hays, Elizabeth/D-3257-2012; OI Dingus, Brenda/0000-0001-8451-7450 FU National Science Foundation [PHY-0245234, PHY-0302000, PHY-0400424, PHY-0504201, PHY-0601080, PHY-0970134, ATM-0002744]; US Department of Energy (Office of High-Energy Physics); US Department of Energy (Office of Nuclear Physics); Los Alamos National Laboratory; University of California; Institute of Geophysics and Planetary Physics FX We gratefully acknowledge Scott Delay and Michael Schneider for their dedicated efforts in the construction and maintenance of the Milagro experiment. This work has been supported by the National Science Foundation (under grants PHY-0245234, -0302000, -0400424, -0504201, -0601080, -0970134, and ATM-0002744), the US Department of Energy (Office of High-Energy Physics and Office of Nuclear Physics), Los Alamos National Laboratory, the University of California, and the Institute of Geophysics and Planetary Physics. NR 26 TC 1 Z9 1 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2012 VL 753 IS 2 AR L31 DI 10.1088/2041-8205/753/2/L31 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967JG UT WOS:000305902700006 ER PT J AU Liszt, H Sonnentrucker, P Cordiner, M Gerin, M AF Liszt, Harvey Sonnentrucker, Paule Cordiner, Martin Gerin, Maryvonne TI THE ABUNDANCE OF C3H2 AND OTHER SMALL HYDROCARBONS IN THE DIFFUSE INTERSTELLAR MEDIUM SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: clouds; ISM: molecules ID CONTINUUM SOURCES; COMPARATIVE CHEMISTRY; MOLECULAR-HYDROGEN; CLOUDS; TRANSLUCENT; ABSORPTION; EMISSION; CARRIER; BAND; CARBON AB Hydrocarbons are ubiquitous in the interstellar medium, observed in diverse environments ranging from diffuse to molecular dark clouds and strong photon-dominated regions near H ii regions. Recently, two broad diffuse interstellar bands (DIBs) at 4881 angstrom and 5450 angstrom were attributed to the linear version of propynylidene l-C3H2, a species whose more stable cyclic conformer c-C3H2 has been widely observed in the diffuse interstellar medium at radio wavelengths. This attribution has already been criticized on the basis of indirect plausibility arguments because the required column densities are quite large, N(l-C3H2)/EB-V = 4 x 10(14) cm (2) mag (1). Here we present new measurements of N(l-C3H2) based on simultaneous 18-21 GHz Very Large Array absorption profiles of cyclic and linear C3H2 taken along sight lines toward extragalactic radio-continuum background sources with foreground Galactic reddening EB-V = 0.1-1.6 mag. We find that N(l-C3H2)/N(c-C3H2) approximate to 1/15-1/40 and N(l-C3H2)/EB-V approximate to (2 +/- 1) x 10(11) cm(-2) mag(-1), so that the column densities of l-C3H2 needed to explain the DIBs are some three orders of magnitude higher than what is observed. We also find N(C4H)/EB-V < 1.3 x 10(13) cm(-2) mag(-1) and N(C4H-)/EB-V < 1 x 10(11) cm(-2) mag(-1) (3 sigma). Using available data for CH and C2H we compare the abundances of small hydrocarbons in diffuse and dark clouds as a guide to their ability to contribute as DIB carriers over a wide range of conditions in the interstellar medium. C1 [Liszt, Harvey] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Sonnentrucker, Paule] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Cordiner, Martin] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20770 USA. [Cordiner, Martin] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20770 USA. [Gerin, Maryvonne] UPMC, Ecole Normale Super, Observ Paris, LERMA,CNRS,UMR 8112, Paris, France. [Gerin, Maryvonne] UCP, Paris, France. RP Liszt, H (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM hliszt@nrao.edu FU French Agence Nationale de la Recherche [ANR-09-BLAN-0231-01]; NASA Astrobiology Institute through Goddard Center for Astrobiology FX The National Radio Astronomy Observatory is operated by Associated Universities, Inc. under a contract with the National Science Foundation. H. L. and M. G. were partially funded by the grant ANR-09-BLAN-0231-01 from the French Agence Nationale de la Recherche as part of the SCHISM project (http://schism.ens.fr/). M. A. C. acknowledges support from the NASA Astrobiology Institute through the Goddard Center for Astrobiology. NR 39 TC 17 Z9 17 U1 1 U2 17 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 JUL 10 PY 2012 VL 753 IS 2 AR L28 DI 10.1088/2041-8205/753/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967JG UT WOS:000305902700003 ER PT J AU Oliveros, JCM Hudson, HS Hurford, GJ Krucker, S Lin, RP Lindsey, C Couvidat, S Schou, J Thompson, WT AF Oliveros, Juan-Carlos Martinez Hudson, Hugh S. Hurford, Gordon J. Krucker, Saem Lin, R. P. Lindsey, Charles Couvidat, Sebastien Schou, Jesper Thompson, W. T. TI THE HEIGHT OF A WHITE-LIGHT FLARE AND ITS HARD X-RAY SOURCES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: flares; Sun: photosphere ID SOLAR-FLARE; PARTICLE-ACCELERATION; RHESSI; ENERGETICS; EMISSIONS; EVENTS; MODELS; YOHKOH; PHASE; EUV AB We describe observations of a white-light (WL) flare (SOL2011-02-24T07:35:00, M3.5) close to the limb of the Sun, from which we obtain estimates of the heights of the optical continuum sources and those of the associated hard X-ray (HXR) sources. For this purpose, we use HXR images from the Reuven Ramaty High Energy Spectroscopic Imager and optical images at 6173 angstrom from the Solar Dynamics Observatory. We find that the centroids of the impulsive-phase emissions in WL and HXRs (30-80 keV) match closely in central distance (angular displacement from Sun center), within uncertainties of order 0 ''.2. This directly implies a common source height for these radiations, strengthening the connection between visible flare continuum formation and the accelerated electrons. We also estimate the absolute heights of these emissions as vertical distances from Sun center. Such a direct estimation has not been done previously, to our knowledge. Using a simultaneous 195 angstrom image from the Solar-Terrestrial RElations Observatory spacecraft to identify the heliographic coordinates of the flare footpoints, we determine mean heights above the photosphere (as normally defined; tau = 1 at 5000 angstrom) of 305 +/- 170 km and 195 +/- 70 km, respectively, for the centroids of the HXR and WL footpoint sources of the flare. These heights are unexpectedly low in the atmosphere, and are consistent with the expected locations of tau = 1 for the 6173 angstrom and the similar to 40 keV photons observed, respectively. C1 [Oliveros, Juan-Carlos Martinez; Hudson, Hugh S.; Hurford, Gordon J.; Krucker, Saem; Lin, R. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Hudson, Hugh S.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Hurford, Gordon J.; Krucker, Saem] Univ Appl Sci N Western Switzerland, Inst Technol 4D, Sch Engn, CH-5210 Windisch, Switzerland. [Lin, R. P.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Lin, R. P.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea. [Lindsey, Charles] NW Res Associates Inc, CORA Div, Boulder, CO USA. [Couvidat, Sebastien; Schou, Jesper] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Thompson, W. T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. RP Oliveros, JCM (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. OI Martinez Oliveros, Juan Carlos/0000-0002-2587-1342 FU NASA [NAS5-98033, NAS5-02139]; WCU [R31-10016]; Korean Ministry of Education, Science, and Technology FX This work was supported by NASA under contract NAS5-98033 for RHESSI for authors Hudson, Hurford, Krucker, Lin, and Martinez Oliveros. R. Lin was also supported in part by the WCU Grant (R31-10016) funded by the Korean Ministry of Education, Science, and Technology. Jesper Schou and Sebastien Couvidat are supported by NASA Contract NAS5-02139 to Stanford University. The HMI data used are courtesy of NASA/SDO and the HMI science team. We thank Martin Fivian for helpful discussions of the RHESSI aspect system. Alex Zehnder's precise metrology of RHESSI has made this analysis possible in the first place. We further thank M. Waltham for comments on the saturation properties of the SECCHI CCD detectors. NR 34 TC 31 Z9 31 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2012 VL 753 IS 2 AR L26 DI 10.1088/2041-8205/753/2/L26 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967JG UT WOS:000305902700001 ER PT J AU Wayth, RB Tingay, SJ Deller, AT Brisken, WF Thompson, DR Wagstaff, KL Majid, WA AF Wayth, Randall B. Tingay, Steven J. Deller, Adam T. Brisken, Walter F. Thompson, David R. Wagstaff, Kiri L. Majid, Walid A. TI LIMITS ON THE EVENT RATES OF FAST RADIO TRANSIENTS FROM THE V-FASTR EXPERIMENT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: observational; pulsars: general; radio continuum: general ID SOFTWARE CORRELATOR; ARRAY; EFFICIENT; PULSARS AB We present the first results from the V-FASTR experiment, a commensal search for fast transient radio bursts using the Very Long Baseline Array (VLBA). V-FASTR is unique in that the widely spaced VLBA antennas provide a discriminant against non-astronomical signals and a mechanism for the localization and identification of events that is not possible with single dishes or short baseline interferometers. Thus, far V-FASTR has accumulated over 1300 hr of observation time with the VLBA, between 90 cm and 3 mm wavelength (327 MHz-86 GHz), providing the first limits on fast transient event rates at high radio frequencies (>1.4 GHz). V-FASTR has blindly detected bright individual pulses from seven known pulsars but has not detected any single-pulse events that would indicate high-redshift impulsive bursts of radio emission. At 1.4 GHz, V-FASTR puts limits on fast transient event rates comparable with the PALFA survey at the Arecibo telescope, but generally at lower sensitivities, and comparable to the "fly's eye" survey at the Allen Telescope Array, but with less sky coverage. We also illustrate the likely performance of the Phase 1 SKA dish array for an incoherent fast transient search fashioned on V-FASTR. C1 [Wayth, Randall B.; Tingay, Steven J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Deller, Adam T.] ASTRON, NL-7991 PD Dwingeloo, Netherlands. [Brisken, Walter F.] NRAO, Socorro, NM 87801 USA. [Thompson, David R.; Wagstaff, Kiri L.; Majid, Walid A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wayth, RB (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM randall.wayth@icrar.org RI Wayth, Randall/B-2444-2013; Tingay, Steven/B-5271-2013; OI Wayth, Randall/0000-0002-6995-4131; Thompson, David/0000-0001-8518-6307; Deller, Adam/0000-0001-9434-3837; Wagstaff, Kiri/0000-0003-4401-5506 FU State Government of Western Australia; Western Australian Centre of Excellence in Radio Astronomy Science and Engineering; NRAO Jansky Fellowship; NWO Veni Fellowship FX The International Centre for Radio Astronomy Research is a Joint Venture between Curtin University and The University of Western Australia, funded by the State Government of Western Australia and the Joint Venture partners. S.J.T is a Western Australian Premiers Research Fellow. R. B. W is supported via the Western Australian Centre of Excellence in Radio Astronomy Science and Engineering. A. T. D was supported by an NRAO Jansky Fellowship and an NWO Veni Fellowship. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the US National Aeronautics and Space Administration. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of NASA's Astrophysics Data System. We thank the anonymous referee for very useful comments that improved the paper. NR 24 TC 13 Z9 13 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 JUL 10 PY 2012 VL 753 IS 2 AR L36 DI 10.1088/2041-8205/753/2/L36 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 967JG UT WOS:000305902700011 ER PT J AU Pavlov, AA Vasilyev, G Ostryakov, VM Pavlov, AK Mahaffy, P AF Pavlov, A. A. Vasilyev, G. Ostryakov, V. M. Pavlov, A. K. Mahaffy, P. TI Degradation of the organic molecules in the shallow subsurface of Mars due to irradiation by cosmic rays SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID AMINO-ACIDS; RADIATION; PRESERVATION; SPECTRA; PROTON; MODEL AB Detection of the organic matter on Mars is one of the main goals of the future Martian landing missions. Yet, the degradation of organic molecules by cosmic ray irradiation on Mars is often ignored. We calculate the radiation dose accumulation rates from solar and galactic cosmic rays at various depths in the shallow Martian subsurface. We demonstrate that a 1-billion-year outcrop on Mars accumulates the dosage of similar to 500 MGy in the top 0-2 cm and similar to 50 MGy at 5-10 cm depths. We show that the preservation of ancient complex organic molecules in the shallow (similar to 10 cm depth) subsurface of rocks could be highly problematic if the exposure age of a geologic outcrop would exceed 300 Myr. We demonstrate that more simple organic molecules with masses similar to 100 amu should have a good chance to survive in the shallow subsurface of rocks. Implications to the sampling strategy for the oncoming Martian missions are discussed. Citation: Pavlov, A. A., G. Vasilyev, V. M. Ostryakov, A. K. Pavlov, and P. Mahaffy (2012), Degradation of the organic molecules in the shallow subsurface of Mars due to irradiation by cosmic rays, Geophys. Res. Lett., 39, L13202, doi:10.1029/2012GL052166. C1 [Pavlov, A. A.; Mahaffy, P.] NASA Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA. [Vasilyev, G.; Pavlov, A. K.] Russian Acad Sci, Lab Mass Spectrometry, Ioffe Phys Tech Inst, St Petersburg, Russia. [Ostryakov, V. M.] St Petersburg State Tech Univ, Phys Tech Dept, St Petersburg, Russia. RP Pavlov, AA (reprint author), NASA Goddard Space Flight Ctr, Planetary Environm Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM alexander.pavlov@nasa.gov RI Pavlov, Alexander/F-3779-2012; Vasilyev, Gennady/E-4843-2014 OI Pavlov, Alexander/0000-0001-8771-1646; FU NASA Exobiology [08-EXOB08-0087]; CRDF [RUP1-2944-ST-09]; Ministry of Education and Science of Russian Federation [11.G34.31.0001] FX This work was partially supported by NASA Exobiology grant 08-EXOB08-0087, CRDF grant RUP1-2944-ST-09, Ministry of Education and Science of Russian Federation contract 11.G34.31.0001. NR 22 TC 40 Z9 40 U1 5 U2 44 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 7 PY 2012 VL 39 AR L13202 DI 10.1029/2012GL052166 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 971WL UT WOS:000306236000003 ER PT J AU Ackermann, M Ajello, M Albert, A Baldini, L Barbiellini, G Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Brigida, M Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J D'Ammando, F de Palma, F Dermer, CD Silva, EDE Drell, PS Drlica-Wagner, A Edmonds, Y Essig, R Favuzzi, C Fegan, SJ Focke, WB Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Guiriec, S Gustafsson, M Hadasch, D Hayashida, M Horan, D Hughes, RE Kamae, T Knodlseder, J Kuss, M Lande, J Lionetto, AM Garde, ML Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Norris, JP Nuss, E Ohsugi, T Okumura, A Orlando, E Ormes, JF Paneque, D Panetta, JH Pesce-Rollins, M Piron, F Pivato, G Porter, TA Prokhorov, D Raino, S Rando, R Razzano, M Reimer, O Roth, M Sbarra, C Scargle, JD Sgro, C Siskind, EJ Snyder, A Spinelli, P Suson, DJ Takahashi, H Tanaka, T Thayer, JG Thayer, JB Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Yang, Z Zimmer, S AF Ackermann, M. Ajello, M. Albert, A. Baldini, L. Barbiellini, G. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Brigida, M. Buehler, R. Buson, S. A. Caliandro, G. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. D'Ammando, F. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Edmonds, Y. Essig, R. Favuzzi, C. Fegan, S. J. Focke, W. B. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Guiriec, S. Gustafsson, M. Hadasch, D. Hayashida, M. Horan, D. Hughes, R. E. Kamae, T. Knoedlseder, J. Kuss, M. Lande, J. Lionetto, A. M. Garde, M. Llena Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Prokhorov, D. Raino, S. Rando, R. Razzano, M. Reimer, O. Roth, M. Sbarra, C. Scargle, J. D. Sgro, C. Siskind, E. J. Snyder, A. Spinelli, P. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Yang, Z. Zimmer, S. CA FERMI-LAT TI Fermi LAT search for dark matter in gamma-ray lines and the inclusive photon spectrum SO PHYSICAL REVIEW D LA English DT Article ID LARGE-AREA TELESCOPE; MILKY-WAY HALO; CONSTRAINTS; ANNIHILATION; MASS; LIKELIHOOD; PHYSICS; MODELS AB Dark matter particle annihilation or decay can produce monochromatic gamma-ray lines and contribute to the diffuse gamma-ray background. Flux upper limits are presented for gamma-ray spectral lines from 7 to 200 GeV and for the diffuse gamma-ray background from 4.8 GeV to 264 GeV obtained from two years of Fermi Large Area Telescope data integrated over most of the sky. We give cross-section upper limits and decay lifetime lower limits for dark matter models that produce gamma-ray lines or contribute to the diffuse spectrum, including models proposed as explanations of the PAMELA and Fermi cosmic-ray data. C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Edmonds, Y.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Prokhorov, D.; Reimer, O.; Snyder, A.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Edmonds, Y.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Prokhorov, D.; Reimer, O.; Snyder, A.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Baldini, L.; Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bonamente, E.; Cecchi, C.; D'Ammando, F.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Buson, S.; Gustafsson, M.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [A. Caliandro, G.; Hadasch, D.; Torres, D. F.] IEEE CSIC, Inst Ciencies Espai, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,CEA IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ciprini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Conrad, J.; Garde, M. Llena; Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Garde, M. Llena; Yang, Z.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy. [D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [Essig, R.] SUNY Stony Brook, CN Yang Inst Theoret Phys, Stony Brook, NY 11794 USA. [Essig, R.] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France. [Lionetto, A. M.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Lionetto, A. M.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Razzano, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Razzano, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Troja, E.] NASA, Postdoctoral Program, Washington, DC USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM elliott@slac.stanford.edu; yedmonds@stanford.edu; rouven.essig@stonybrook.edu RI Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Funk, Stefan/B-7629-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852; Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU Fermi LAT; National Aeronautics and Space Administration and the Department of Energy in the United States; Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council and the Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy and the Centre National d' Etudes Spatiales in France FX The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l' Enewwrgie 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. J. Conrad is supported by a grant from the K. A. Wallenberg Foundation.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d' Etudes Spatiales in France. NR 64 TC 150 Z9 150 U1 0 U2 15 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 JUL 5 PY 2012 VL 86 IS 2 AR 022002 DI 10.1103/PhysRevD.86.022002 PG 21 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 971GY UT WOS:000306193000001 ER PT J AU Berman, ESF Fladeland, M Liem, J Kolyer, R Gupta, M AF Berman, Elena S. F. Fladeland, Matthew Liem, Jimmy Kolyer, Richard Gupta, Manish TI Greenhouse gas analyzer for measurements of carbon dioxide, methane, and water vapor aboard an unmanned aerial vehicle SO SENSORS AND ACTUATORS B-CHEMICAL LA English DT Article DE Greenhouse gas; ICOS; UAV; Optical sensor; Carbon dioxide; Methane; Water vapor ID STRATOSPHERE-TROPOSPHERE EXCHANGE; CAVITY; SPECTROSCOPY AB A compact, lightweight atmospheric gas analyzer has been integrated into and flown on the National Aeronautics and Space Administration (NASA) Sensor Integrated Environmental Remote Research Aircraft (SIERRA) unmanned aerial vehicle (UAV) and deployed to make highly accurate, 1 Hz measurements of methane, carbon dioxide, and water vapor. The analyzer was used to measure gas concentrations in flight and to demonstrate the system for providing measurements at altitudes as low as 10 m and in remote locations. The first flights were conducted at Crows Landing, CA, an agricultural site, with H2O concentrations showing distinct structure and sharp features that were well outside of the measurement noise. The instrument was then deployed in Svalbard, Norway prior to the NASA Characterization of Arctic Sea Ice Experiment (CASIE). During the Svalbard flight, there was minimal variation in the CO2 and CH4 concentrations, but the water concentration changed dramatically, oscillating as the aircraft moved repeatedly through its racetrack shaped flight pattern. The regions of high water concentration corresponded to low-lying areas which collect runoff from the nearby Vestre Broggerbreen glacier. This novel, integrated instrument-aircraft system allows more numerous and efficient measurements of carbon dioxide, methane, and water vapor concentrations at low-altitudes and in remote or dangerous locations. (C) 2012 Elsevier B.V. All rights reserved. C1 [Berman, Elena S. F.; Liem, Jimmy; Gupta, Manish] Los Gatos Res, Mountain View, CA 94043 USA. [Fladeland, Matthew; Kolyer, Richard] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Berman, ESF (reprint author), Los Gatos Res, 67 E Evelyn Ave,Suite 3, Mountain View, CA 94043 USA. EM e.berman@lgrinc.com FU NASA SBIR [NNX09CC17P] FX The authors would like to thank all the members of the NASA CASIE team, especially Lesli Monforton, Brad Lobitz, Mark Sumich, Mike Gaunce, Randy Berthold, and Don Herlth. The authors would also like to thank the researchers at the Norwegian Institute for Air Research, especially Ove Hermansen, and researchers at the Department of Applied Environmental Science, Stockholm University, especially Birgitta Noone, for their assistance and the use of their data. This work was supported by NASA SBIR Grant #NNX09CC17P. NR 18 TC 16 Z9 16 U1 3 U2 44 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 JUL 5 PY 2012 VL 169 BP 128 EP 135 DI 10.1016/j.snb.2012.04.036 PG 8 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA 964TM UT WOS:000305719600018 ER PT J AU Liu, CL Allan, RP Huffman, GJ AF Liu, Chunlei Allan, Richard P. Huffman, George J. TI Co-variation of temperature and precipitation in CMIP5 models and satellite observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SURFACE-TEMPERATURE; CLIMATE; SCALES; SSM/I; CYCLE AB Current variability of precipitation (P) and its response to surface temperature (T) are analysed using coupled (CMIP5) and atmosphere-only (AMIP5) climate model simulations and compared with observational estimates. There is striking agreement between Global Precipitation Climatology Project (GPCP) observed and AMIP5 simulated P anomalies over land both globally and in the tropics suggesting that prescribed sea surface temperature and realistic radiative forcings are sufficient for simulating the interannual variability in continental P. Differences between the observed and simulated P variability over the ocean, originate primarily from the wet tropical regions, in particular the western Pacific, but are reduced slightly after 1995. All datasets show positive responses of P to T globally of around 2%/K for simulations and 3-4%/K in GPCP observations but model responses over the tropical oceans are around 3 times smaller than GPCP over the period 1988-2005. The observed anticorrelation between land and ocean P, linked with El Nino Southern Oscillation, is captured by the simulations. All data sets over the tropical ocean show a tendency for wet regions to become wetter and dry regions drier with warming. Over the wet region (>= 75% precipitation percentile), the precipitation response is similar to 13-15%/K for GPCP and similar to 5%/K for models while trends in P are 2.4%/decade for GPCP, 0.6% /decade for CMIP5 and 0.9%/decade for AMIP5 suggesting that models are underestimating the precipitation responses or a deficiency exists in the satellite datasets. Citation: Liu, C., R. P. Allan, and G. J. Huffman (2012), Co-variation of temperature and precipitation in CMIP5 models and satellite observations, Geophys. Res. Lett., 39, L13803, doi: 10.1029/2012GL052093. C1 [Liu, Chunlei; Allan, Richard P.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. [Huffman, George J.] Sci Syst & Applicat Inc, Greenbelt, MD USA. [Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Liu, CL (reprint author), Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. EM c.l.liu@reading.ac.uk RI Allan, Richard/B-5782-2008; Huffman, George/F-4494-2014 OI Allan, Richard/0000-0003-0264-9447; Huffman, George/0000-0003-3858-8308 FU UK Natural Environmental Research Council [NE/I006672/1, NE/G015708/1]; National Centre for Earth Observations; National Centre for Atmospheric Science FX This work was undertaken as part of the PAGODA and PREPARE projects funded by the UK Natural Environmental Research Council under grants NE/I006672/1 and NE/G015708/1 and was supported by the National Centre for Earth Observations and the National Centre for Atmospheric Science. GPCP v2.2 data were extracted from http://precip.gsfc.nasa.gov/gpcp_v2.2_data.html, TMI data from ftp.ssmi.com, TRMM 3B42 data from http://mirador.gsfc.nasa.gov/, and CMIP5 and AMIP5 data sets from the BADC (British Atmospheric Data Centre, http://badc.nerc.ac.uk/home/index.html) and the PCMDI (Program for Climate Model Diagnosis and Intercomparison, http://pcmdi3.llnl.gov/esgcet/home.htm). We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP, and we thank the climate modeling groups (models listed in Table 1) for producing and making available their model output. For CMIP, the U.S. Department of Energy's PCMDI provided coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. The scientists involved in the generation of these data sets are sincerely acknowledged. We sincerely thank the two reviewers for their insightful comments which have helped to improve the paper. NR 27 TC 50 Z9 50 U1 0 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 4 PY 2012 VL 39 AR L13803 DI 10.1029/2012GL052093 PG 8 WC Geosciences, Multidisciplinary SC Geology GA 971WG UT WOS:000306235300004 ER PT J AU Hansell, RA Tsay, SC Hsu, NC Ji, Q Bell, SW Holben, BN Welton, EJ Roush, TL Zhang, W Huang, J Li, ZQ Chen, H AF Hansell, Richard A. Tsay, Si-Chee Hsu, N. Christina Ji, Qiang Bell, Shaun W. Holben, Brent N. Welton, Ellsworth J. Roush, Ted L. Zhang, W. Huang, J. Li, Zhanqing Chen, H. TI An assessment of the surface longwave direct radiative effect of airborne dust in Zhangye, China, during the Asian Monsoon Years field experiment (2008) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-CONSTANTS; AEROSOLS; TEMPERATURE; MINERALS; CALCITE; SYSTEMS; CLOUDS; SAHARA; IMPACT; ROCKS AB In April-June 2008, NASA Goddard's ground-based mobile laboratories (SMART-COMMIT) were deployed to Zhangye China (39.0 degrees N; 101 degrees W) to support the Asian Monsoon Years field experiment and the East Asian Study of Tropospheric Aerosols and Impact on Regional Climate. One of the primary objectives at Zhangye, a semi-arid region located between the Taklimakan and Gobi Deserts, was to capture and characterize dust aerosols near the source and to quantify their direct radiative effects (DRE). A regional dust optical model was constructed by combining previously measured soil mineralogy data at Zhangye with COMMIT's particle microphysical measurements. During a 2-week period of heightened dust activity, retrieved longwave (LW) aerosol optical thickness (tau) from SMART's Atmospheric Emitted Radiance Interferometer was used in the Fu-Liou radiative transfer model to derive LW instantaneous DRE (DRELW) at the surface, top of atmosphere, and heating rate profiles for cloud-free conditions. Conservatively, surface instantaneous DRELW and LW forcing efficiency range from about 2-20 Wm(-2) and 31-35 Wm(-2)tau(-1) (0 <= tau <= 83), respectively. The significance of DRELW relative to its shortwave counterpart was estimated to be between 51 and 58%, but of opposite sign, partly compensating shortwave surface cooling. Compared to Saharan dust observed during the NAMMA-2006 field experiment at Cape Verde, dust LW forcing efficiency for this study was found to be a factor of two larger stemming from differences in environmental and surface conditions, aerosol absorption, and Zhangye's close proximity to major desert sources. Relative to observed and modeled ranges in surface DRELW for clouds (similar to 30-80 Wm(-2)) and greenhouse gases (similar to 2 Wm(-2)), this study's upper range in DRELW represents a significant perturbation to the climate system with important implications for better understanding regional changes in surface temperatures and moisture budgets. C1 [Hansell, Richard A.; Ji, Qiang; Li, Zhanqing] Univ Maryland, ESSIC, College Pk, MD 20740 USA. [Hansell, Richard A.; Tsay, Si-Chee; Hsu, N. Christina; Ji, Qiang; Bell, Shaun W.; Holben, Brent N.; Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bell, Shaun W.] Sci Syst & Applicat Inc, Lanham, MD USA. [Roush, Ted L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zhang, W.; Huang, J.] Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. [Li, Zhanqing] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20740 USA. [Chen, H.] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China. RP Hansell, RA (reprint author), Univ Maryland, ESSIC, College Pk, MD 20740 USA. EM richard.a.hansell@nasa.gov RI Hsu, N. Christina/H-3420-2013; Tsay, Si-Chee/J-1147-2014; Hansell, Richard/J-2065-2014; Li, Zhanqing/F-4424-2010 OI Li, Zhanqing/0000-0001-6737-382X FU NASA's Radiation Sciences Program; NASA Earth Observing System and Radiation Sciences Program FX Our research is supported by NASA's Radiation Sciences Program, managed by Hal B. Maring. We thank our domestic and international partners including DOE's ARM program, the Institute of Atmospheric Physics at Beijing, and Lanzhou University during AMY08. Both AERONET and MPLNET are funded by the NASA Earth Observing System and Radiation Sciences Program. We thank W. Feltz and V. Ossenkopf and M. Mishchenko for making available the AERIPLUS, Effective Medium Calculator, and Mie light-scattering codes, respectively. Figure 1a in this study was produced with the Giovanni online data system, developed and maintained by the NASA GES DISC. Last, we thank the NASA Goddard SMARTLabs team for all of their efforts during the deployment and study and to the anonymous reviewers of this manuscript for their helpful comments and suggestions. NR 66 TC 11 Z9 11 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 4 PY 2012 VL 117 AR D00K39 DI 10.1029/2011JD017370 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 971WS UT WOS:000306237000002 ER PT J AU Hurkmans, RTWL Bamber, JL Sorensen, LS Joughin, IR Davis, CH Krabill, WB AF Hurkmans, R. T. W. L. Bamber, J. L. Sorensen, L. S. Joughin, I. R. Davis, C. H. Krabill, W. B. TI Spatiotemporal interpolation of elevation changes derived from satellite altimetry for Jakobshavn Isbrae, Greenland SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID CONTINENTAL ICE SHEETS; VOLUME CHANGE; MASS-LOSS; RADAR ALTIMETRY; OUTLET GLACIERS; WEST GREENLAND; SEA-LEVEL; VELOCITY; BALANCE; ACCURACY AB Estimation of ice sheet mass balance from satellite altimetry requires interpolation of point-scale elevation change (dH/dt) data over the area of interest. The largest dH/dt values occur over narrow, fast-flowing outlet glaciers, where data coverage of current satellite altimetry is poorest. In those areas, straightforward interpolation of data is unlikely to reflect the true patterns of dH/dt. Here, four interpolation methods are compared and evaluated over Jakobshavn Isbrae, an outlet glacier for which widespread airborne validation data are available from NASA's Airborne Topographic Mapper (ATM). The four methods are ordinary kriging (OK), kriging with external drift (KED), where the spatial pattern of surface velocity is used as a proxy for that of dH/dt, and their spatiotemporal equivalents (ST-OK and ST-KED). KED assumes a linear relationship between spatial gradients of velocity and dH/dt, which is confirmed for both negative (Pearson's correlation rho < -0.85) and, to a lesser degree, positive (rho = 0.73) dH/dt values. When compared to ATM data, KED and ST-KED yield more realistic spatial patterns and higher thinning rates (over 20 m yr(-1) as opposed to 7 m yr(-1) for OK). Spatiotemporal kriging smooths inter-annual variability and improves interpolation in periods with sparse data coverage and we conclude, therefore, that ST-KED produces the best results. Using this method increases volume loss estimates from Jakobshavn Isbrae by up to 20% compared to those obtained by OK. The proposed interpolation method will improve ice sheet mass balance reconstructions from existing and past satellite altimeter data sets, with generally poor sampling of outlet glaciers. C1 [Hurkmans, R. T. W. L.; Bamber, J. L.] Univ Bristol, Sch Geog Sci, Bristol Glaciol Ctr, Bristol BS8 1SS, Avon, England. [Sorensen, L. S.] DTU Space, Geodynam Dept, Copenhagen, Denmark. [Joughin, I. R.] Univ Washington, Polar Sci Ctr, Seattle, WA 98195 USA. [Davis, C. H.] Univ Missouri, Ctr Geospatial Intelligence, Columbia, MO USA. [Krabill, W. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hurkmans, RTWL (reprint author), Univ Bristol, Sch Geog Sci, Bristol Glaciol Ctr, Bristol BS8 1SS, Avon, England. EM ruud.hurkmans@bristol.ac.uk RI Hurkmans, Ruud/B-8286-2012; Bamber, Jonathan/C-7608-2011; Joughin, Ian/A-2998-2008; Sorensen, Louise/E-5282-2014 OI Hurkmans, Ruud/0000-0002-9164-7445; Bamber, Jonathan/0000-0002-2280-2819; Joughin, Ian/0000-0001-6229-679X; Sorensen, Louise/0000-0002-3771-4061 FU European Union [226375] FX This work was supported by funding to the ice2sea programme from the European Union 7th Framework Programme, grant 226375 and Ice2sea contribution 28. We thank the three reviewers and the editor for their thoughtful and constructive comments. NR 51 TC 9 Z9 9 U1 1 U2 15 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 JUL 4 PY 2012 VL 117 AR F03001 DI 10.1029/2011JF002072 PG 16 WC Geosciences, Multidisciplinary SC Geology GA 971SO UT WOS:000306224300001 ER PT J AU Sarantos, M Hartle, RE Killen, RM Saito, Y Slavin, JA Glocer, A AF Sarantos, M. Hartle, R. E. Killen, R. M. Saito, Y. Slavin, J. A. Glocer, A. TI Flux estimates of ions from the lunar exosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SURFACE AB We compare estimates for the ion fluxes of twelve expected constituents of the lunar exosphere with estimates for the ion fluxes ejected from the lunar surface by solar wind ions and electrons. Our estimates demonstrate that measurements of lunar ions will help constrain the abundances of many undetected species in the lunar exosphere, particularly Al and Si, because the expected ion flux levels from the exosphere exceed those from the surface. To correctly infer the relative abundances of exospheric ions and neutrals from Kaguya Ion Mass Analyzer (IMA) measurements, we must take into account the velocity distributions of local ions. The predicted spectrum underestimates the measured levels of O+ relative to other lunar ion species, a result that may suggest contributions by molecular ions to the measured O+ rates. Citation: Sarantos, M., R. E. Hartle, R. M. Killen, Y. Saito, J. A. Slavin, and A. Glocer (2012), Flux estimates of ions from the lunar exosphere, Geophys. Res. Lett., 39, L13101, doi:10.1029/2012GL052001. C1 [Sarantos, M.; Hartle, R. E.; Glocer, A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Sarantos, M.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. [Sarantos, M.; Hartle, R. E.; Killen, R. M.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA. [Killen, R. M.] NASA, Goddard Space Flight Ctr, Planetary Magnetospheres Branch, Greenbelt, MD 20771 USA. [Saito, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Slavin, J. A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Sarantos, M (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Code 670-0, Greenbelt, MD 20771 USA. EM menelaos.sarantos-1@nasa.gov RI Slavin, James/H-3170-2012; Glocer, Alex/C-9512-2012; Sarantos, Menelaos/H-8136-2013 OI Slavin, James/0000-0002-9206-724X; Glocer, Alex/0000-0001-9843-9094; FU NASA Lunar Science Institute, DREAM FX MS, REH, and RMK acknowledge funding from the NASA Lunar Science Institute, DREAM. NR 19 TC 12 Z9 12 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 3 PY 2012 VL 39 AR L13101 DI 10.1029/2012GL052001 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 971WF UT WOS:000306235100004 ER PT J AU Jorba, O Dabdub, D Blaszczak-Boxe, C Perez, C Janjic, Z Baldasano, JM Spada, M Badia, A Goncalves, M AF Jorba, O. Dabdub, D. Blaszczak-Boxe, C. Perez, C. Janjic, Z. Baldasano, J. M. Spada, M. Badia, A. Goncalves, M. TI Potential significance of photoexcited NO2 on global air quality with the NMMB/BSC chemical transport model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CONVECTIVE ADJUSTMENT SCHEME; ATMOSPHERIC CHEMISTRY; EXCITED NO2; OZONE; HONO; PARAMETERIZATION; COORDINATE; IMPACTS; ENERGY; H2O AB Atmospheric chemists have recently focused on the relevance of the NO2* + H2O -> OH + HONO reaction to local air quality. This chemistry has been considered not relevant for the troposphere from known reaction rates until nowadays. New experiments suggested a rate constant of 1.7 x 10(-13) cm(3) molecule(-1) s(-1), which is an order of magnitude faster than the previously estimated upper limit of 1.2 x 10(-14) cm(3) molecule(-1) s(-1), determined by Crowley and Carl (1997). Using the new global model, NMMB/BSC Chemical Transport Model (NMMB/BSC-CTM), simulations are presented that assess the potential significance of this chemistry on global air quality. Results show that if the NO2* chemistry is considered following the upper limit kinetics recommended by Crowley and Carl (1997), it produces an enhancement of ozone surface concentrations of 4-6 ppbv in rural areas and 6-15 ppbv in urban locations, reaching a maximum enhancement of 30 ppbv in eastern Asia. Moreover, NO2 enhancements are minor (<0.01 ppbv) in background regions and reach maximum daytime values of 1-6 ppbv. Similarly, HONO exhibits negligible increases, 8-9 pptv in urban settings. Enhancements in the concentration of OH are around 14-17 x 10(5) molec cm(-3). Decreases in the concentration of O-3 and its precursors are also identified but to a lesser degree. In order to quantify the role of the two kinetic rates measured, model simulations are compared after incorporating both reaction rate constants. Maximum O-3 difference enhancements from 5 to 10 ppbv are modeled over locations where high NOx emissions are present; however, differences are small in most parts of the globe. C1 [Jorba, O.; Baldasano, J. M.; Spada, M.; Badia, A.; Goncalves, M.] Barcelona Supercomp Ctr, Dept Earth Sci, ES-08034 Barcelona, Spain. [Dabdub, D.] Univ Calif Irvine, Dept Mech & Aerosp Engn, Irvine, CA 92717 USA. [Blaszczak-Boxe, C.] CUNY, Dept Phys Environm & Comp Sci, Medgar Evers Coll, New York, NY 10021 USA. [Perez, C.] NASA Goddard Inst Space Studies, New York, NY USA. [Perez, C.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Janjic, Z.] Natl Ctr Environm Predict, Camp Springs, MD USA. [Baldasano, J. M.; Goncalves, M.] Tech Univ Catalonia, Projects Dept, Environm Modeling Lab, Barcelona, Spain. RP Jorba, O (reprint author), Barcelona Supercomp Ctr, Dept Earth Sci, Jordi Girona 31, ES-08034 Barcelona, Spain. EM oriol.jorba@bsc.es RI Goncalves-Ageitos, Maria/H-2130-2015; OI Goncalves-Ageitos, Maria/0000-0003-3857-6403; Perez Garcia-Pando, Carlos/0000-0002-4456-0697; Jorba, Oriol/0000-0001-5872-0244 FU Spanish Ministry of Economy and Competitiveness [CGL2008-02818-CLI, CGL2010-19652] FX The authors wish to thank WOUDC, GAW, EMEP, CASTNET-EPA for the provision of measurement stations. Also, thanks to S. Szopa and A. Cozic for the provision of LMDz-INCA2 chemical data as initial chemical conditions. This work is funded by grants CGL2008-02818-CLI and CGL2010-19652 of the Spanish Ministry of Economy and Competitiveness. All the numerical simulations were performed with the MareNostrum Supercomputer hosted by the Barcelona Supercomputing Center. NR 54 TC 14 Z9 14 U1 0 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 3 PY 2012 VL 117 AR D13301 DI 10.1029/2012JD017730 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 971WQ UT WOS:000306236800005 ER PT J AU Cady, E AF Cady, Eric TI Boundary diffraction wave integrals for diffraction modeling of external occulters SO OPTICS EXPRESS LA English DT Article ID MAGGI-RUBINOWICZ THEORY; PLANETS AB An occulter is a large diffracting screen which may be flown in conjunction with a telescope to image extrasolar planets. The edge is shaped to minimize the diffracted light in a region beyond the occulter, and a telescope may be placed in this dark shadow to view an extrasolar system with the starlight removed. Errors in position, orientation, and shape of the occulter will diffract additional light into this region, and a challenge of modeling an occulter system is to accurately and quickly model these effects. We present a fast method for the calculation of electric fields following an occulter, based on the concept of the boundary diffraction wave: the 2D structure of the occulter is reduced to a 1D edge integral which directly incorporates the occulter shape, and which can be easily adjusted to include changes in occulter position and shape, as well as the effects of sources-such as exoplanets-which arrive off-axis to the occulter. The structure of a typical implementation of the algorithm is included. (C) 2012 Optical Society of America C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cady, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM eric.j.cady@jpl.nasa.gov FU NASA FX This work was carried out as a part of the Imaging Performance Study funded by NASA's Exoplanet Exploration Program; the research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 16 TC 8 Z9 9 U1 10 U2 10 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUL 2 PY 2012 VL 20 IS 14 BP 15196 EP 15208 DI 10.1364/OE.20.015196 PG 13 WC Optics SC Optics GA 971BF UT WOS:000306176100060 PM 22772218 ER PT J AU Chen, JR Numata, K Wu, ST AF Chen, Jeffrey R. Numata, Kenji Wu, Stewart T. TI Error reduction methods for integrated-path differential-absorption lidar measurements SO OPTICS EXPRESS LA English DT Article ID ATMOSPHERIC CO2; SPECTRAL REFLECTANCE; CARBON-DIOXIDE; MU-M; SENSITIVITY; MISSION; NOISE; SHAPE AB We report new modeling and error reduction methods for differential-absorption optical-depth (DAOD) measurements of atmospheric constituents using direct-detection integrated-path differential-absorption lidars. Errors from laser frequency noise are quantified in terms of the line center fluctuation and spectral line shape of the laser pulses, revealing relationships verified experimentally. A significant DAOD bias is removed by introducing a correction factor. Errors from surface height and reflectance variations can be reduced to tolerable levels by incorporating altimetry knowledge and "log after averaging", or by pointing the laser and receiver to a fixed surface spot during each wavelength cycle to shorten the time of "averaging before log". (C) 2012 Optical Society of America C1 [Chen, Jeffrey R.; Numata, Kenji; Wu, Stewart T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Chen, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jeffrey.r.chen@nasa.gov FU NASA Goddard Internal Research and Development program; NASA Earth Science Technology Office Instrument Incubator Program FX The authors gratefully acknowledge Dr. J. Mao and Dr. X. Sun of NASA Goddard for fruitful discussions and help in atmospheric modeling and lidar link budget calculations. They are also indebted to Dr. A. Amediek of Deutsches Zentrum fur Luft- und Raumfahrt (DLR) for sharing surface reflectance measurement data, Dr. J. Abshire and other members of the Goddard CO2 sounder team for their support. This work was supported by the NASA Goddard Internal Research and Development program and the NASA Earth Science Technology Office Instrument Incubator Program. NR 29 TC 6 Z9 6 U1 1 U2 10 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUL 2 PY 2012 VL 20 IS 14 BP 15589 EP 15609 DI 10.1364/OE.20.015589 PG 21 WC Optics SC Optics GA 971BF UT WOS:000306176100096 PM 22772254 ER PT J AU Siegel, PH AF Siegel, Peter H. TI Untitled 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.] JPL, Pasadena, CA USA. RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA. EM phs@caltech.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD JUL PY 2012 VL 2 IS 4 BP 373 EP 376 DI 10.1109/TTHZ.2012.2204350 PG 4 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AG UT WOS:000318767400001 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 91109 USA. [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91109 USA. [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD JUL PY 2012 VL 2 IS 4 BP 377 EP 377 DI 10.1109/TTHZ.2012.2198215 PG 1 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AG UT WOS:000318767400002 ER PT J AU Goldsmith, PF Lis, DC AF Goldsmith, Paul F. Lis, Dariusz C. TI Early Science Results From the Heterodyne Instrument for the Far Infrared (HIFI) on the Herschel Space Observatory SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Submillimeter wave technology; astrophysics; astrochemistry; star formation ID EXTRAORDINARY SOURCES HEXOS; WAVE-ASTRONOMY-SATELLITE; STAR-FORMING REGIONS; HYDROGEN-FLUORIDE; MOLECULAR CLOUDS; SAGITTARIUS B2(M); INTERSTELLAR OH+; DIFFUSE CLOUDS; WATER-VAPOR; LINE SURVEY AB The Heterodyne Instrument for the Far Infrared (HIFI) on the Herschel Space Observatory covers 480 to 1250 GHz and 1410 to 1910 GHz for high spectral resolution astronomical spectroscopy. Herschel was launched on 14 May 2009, and following cooldown and commissioning, HIFI has been used along with the other two focal plane instruments for a wide variety of astronomical observations. These have ranged from studies of the structure of the interstellar medium in nearby galaxies to detailed studies of the chemistry in star-forming regions of the Milky Way. Observations of the solar system have yielded new results about water in comets and its relationship to the Earth's oceans. In this paper, following a brief review of the instrument and its performance, we give an overview of the most important HIFI discoveries to date. This is necessarily very selective, but is intended to give a hint of the results obtained with this instrument that has really opened submillimeter wavelengths for high-sensitivity/high-resolution spectroscopy. C1 [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lis, Dariusz C.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Paul.F.Goldsmith@jpl.nasa.gov; dcl@caltech.edu RI Goldsmith, Paul/H-3159-2016 NR 64 TC 4 Z9 4 U1 1 U2 4 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 JUL PY 2012 VL 2 IS 4 BP 383 EP 392 DI 10.1109/TTHZ.2012.2200553 PG 10 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 142AG UT WOS:000318767400004 ER PT J AU Hah, C Shin, HW AF Hah, Chunill Shin, Hyoun-Woo TI Study of Near-Stall Flow Behavior in a Modern Transonic Fan With Compound Sweep SO JOURNAL OF FLUIDS ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article ID TIP CLEARANCE; COMPRESSOR AB Detailed flow behavior in a modern transonic fan with a compound sweep is investigated in this paper. Both unsteady Reynolds-averaged Navier-Stokes (URANS) and large eddy simulation (LES) methods are applied to investigate the flow field over a wide operating range. The calculated flow fields are compared with the data from an array of high-frequency response pressure transducers embedded in the fan casing. The current study shows that a relatively fine computational grid is required to resolve the flow field adequately and to calculate the pressure rise across the fan correctly. The calculated flow field shows detailed flow structure near the fan rotor tip region. Due to the introduction of compound sweep toward the rotor tip, the flow structure at the rotor tip is much more stable compared to that of the conventional blade design. The passage shock stays very close to the leading edge at the rotor tip even at the throttle limit. On the other hand, the passage shock becomes stronger and detaches earlier from the blade passage at the radius where the blade sweep is in the opposite direction. The interaction between the tip clearance vortex and the passage shock becomes intense as the fan operates toward the stall limit, and tip clearance vortex breakdown occurs at near-stall operation. URANS calculates the time-averaged flow field fairly well. Details of measured rms static pressure are not calculated with sufficient accuracy with URANS. On the other hand, LES calculates details of the measured unsteady flow features in the current transonic fan with compound sweep fairly well and reveals the flow mechanism behind the measured unsteady flow field. [DOI: 10.1115/1.4006878] C1 [Hah, Chunill] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Shin, Hyoun-Woo] GE Aviat, Aero Technol Lab, Cincinnati, OH 45215 USA. RP Hah, C (reprint author), NASA, Glenn Res Ctr, MS 5-11,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Chunill.Hah-1@nasa.gov; hyoun-woo.shin@ge.com NR 16 TC 8 Z9 9 U1 1 U2 5 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0098-2202 J9 J FLUID ENG-T ASME JI J. Fluids Eng.-Trans. ASME PD JUL PY 2012 VL 134 IS 7 AR 071101 DI 10.1115/1.4006878 PG 7 WC Engineering, Mechanical SC Engineering GA 087KF UT WOS:000314759500001 ER PT J AU Goldberg, RK Blinzler, BJ Binienda, WK AF Goldberg, Robert K. Blinzler, Brina J. Binienda, Wieslaw K. TI Modification of a Macromechanical Finite Element-Based Model for Impact Analysis of Triaxially Braided Composites SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE Composite; Impact; High strain rate; Braid; Containment; Finite-element analysis; Macro scale ID TEXTILE COMPOSITES; FIBER-COMPOSITES; BEHAVIOR AB A macrolevel finite element-based model has been developed to simulate the mechanical and impact response of triaxially braided polymer matrix composites. In the analytical model, the triaxial-braid architecture is simulated by using four parallel shell elements, each of which is modeled as a laminated composite. For the current analytical approach, each shell element is considered to be a smeared homogeneous material. The commercial transient dynamic finite-element code LS-DYNA is used to conduct the simulations, and a continuum damage mechanics model internal to LS-DYNA is used as the material constitutive model. The constitutive model requires stiffness and strength properties of an equivalent unidirectional composite. Simplified micromechanics methods are used to determine the equivalent stiffness properties, and results from coupon-level tests on the braided composite are utilized to back out the required strength properties. Simulations of quasi-static coupon tests of several representative braided composites are conducted to demonstrate the correlation of the model. Impact simulations of a represented braided composite are conducted to demonstrate the capability of the model to predict the penetration velocity and damage patterns obtained experimentally. DOI: 10.1061/(ASCE)AS.1943-5525.0000135. (C) 2012 American Society of Civil Engineers. C1 [Goldberg, Robert K.] NASA, Glenn Res Ctr, Mech & Life Predict Branch, Cleveland, OH 44135 USA. [Blinzler, Brina J.; Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. RP Blinzler, BJ (reprint author), Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA. EM bjc43@zips.uakron.edu FU Aging Aircraft and Durability Program of the Aviation Safety Project FX This work was funded by the Aging Aircraft and Durability Program of the Aviation Safety Project. NR 18 TC 4 Z9 4 U1 3 U2 16 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2012 VL 25 IS 3 BP 383 EP 394 DI 10.1061/(ASCE)AS.1943-5525.0000135 PG 12 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 066RV UT WOS:000313238800006 ER PT J AU Achberger, C Ackerman, SA Ahmed, FH Albanil-Encarnacion, A Alfaro, EJ Alves, LM Allan, R Amador, JA Ambenje, P Antoine, MD Antonov, J Arevalo, J Arndt, DS Ashik, I Atheru, Z Baccini, A Baez, J Banzon, V Baringer, MO Barreira, S Barriopedro, DE Bates, JJ Becker, A Behrenfeld, MJ Bell, GD Benedetti, A Bernhard, G Berrisford, P Berry, DI Beszczynska-Moeller, A Bhatt, US Bidegain, M Bieniek, P Birkett, C Bissolli, P Blake, ES Blunden, J Boudet-Rouco, D Box, JE Boyer, T Braathen, GO Brackenridge, GR Brohan, P Bromwich, DH Brown, L Brown, R Bruhwiler, L Bulygina, ON Burrows, J Calderon, B Camargo, SJ Cappellen, J Carmack, E Carrasco, G Chambers, DP Christiansen, HH Christy, J Chung, D Ciais, P Coehlo, CAS Colwell, S Comiso, J Cretaux, JF Crouch, J Cunningham, SA De Jeu, RAM Demircan, M Derksen, C Diamond, HJ Dlugokencky, EJ Dohan, K Dolman, AJ Dorigo, WA Drozdov, DS Duguay, C Dutton, E Dutton, GS Elkins, JW Epstein, HE Famiglietti, JS Fanton d'Andon, OH Feely, RA Fekete, BM Fenimore, C Fernandez-Prieto, D Fields, E Fioletov, V Fogt, RL Folland, C Foster, MJ Frajka-Williams, E Franz, BA Frey, K Frith, SH Frolov, I Frost, GV Ganter, C Garzoli, S Gitau, W Gleason, KL Gobron, N Goldenberg, SB Goni, G Gonzalez-Garcia, I Gonzalez-Rodriguez, N Good, SA Goryl, P Gottschalck, J Gouveia, CM Gregg, MC Griffiths, GM Grigoryan, V Grooss, JU Guard, C Guglielmin, M Hall, BD Halpert, MS Heidinger, AK Heikkila, A Heim, RR Hennon, PA Hidalgo, HG Hilburn, K Ho, SP Hobbs, WR Holgate, S Hook, SJ Hovsepyan, A Hu, ZZ Hugony, S Hurst, DF Ingvaldsen, R Itoh, M Jaimes, E Jeffries, M Johns, WE Johnsen, B Johnson, B Johnson, GC Jones, LT Jumaux, G Kabidi, K Kaiser, JW Kang, KK Kanzow, TO Kao, HY Keller, LM Kendon, M Kennedy, JJ Kervankiran, S Key, J Khatiwala, S Kholodov, AL Khoshkam, M Kikuchi, T Kimberlain, TB King, D Knaff, JA Korshunova, NN Koskela, T Kratz, DP Krishfield, R Kruger, A Kruk, MC Kumar, A Lagerloef, G Lakkala, K Lammers, RB Lander, MA Landsea, CW Lankhorst, M Lapinel-Pedroso, B Lazzara, MA LeDuc, S Lefale, P Leon, G Leon-Lee, A Leuliette, E Levitus, S L'Heureux, M Lin, II Liu, HX Liu, YJ Liu, Y Lobato-Sanchez, R Locarnini, R Loeb, NG Loeng, H Long, CS Lorrey, AM Lumpkin, R Myhre, CL Luo, JJ Lyman, JM MacCallum, S Macdonald, AM Maddux, BC Manney, G Marchenko, SS Marengo, JA Maritorena, S Marotzke, J Marra, JJ Martinez-Sanchez, O Maslanik, J Massom, RA Mathis, JT McBride, C McClain, CR McGrath, D McGree, S McLaughlin, F McVicar, TR Mears, C Meier, W Meinen, CS Menendez, M Merchant, C Merrifield, MA Miller, L Mitchum, GT Montzka, SA Moore, S Mora, NP Morcrette, JJ Mote, T Muhle, J Mullan, AB Muller, R Myhre, C Nash, ER Nerem, RS Newlin, ML Newman, PA Ngari, A Nishino, S Njau, LN Noetzli, J Oberman, NG Obregon, A Ogallo, L Oludhe, C Overland, J Oyunjargal, L Parinussa, RM Park, GH Parker, DE Pasch, RJ Pascual-Ramirez, R Pelto, MS Penalba, O Perez-Suarez, R Perovich, D Pezza, AB Phillips, D Pickart, R Pinty, B Pinzon, J Pitts, MC Pour, HK Prior, J Privette, JL Proshutinsky, A Quegan, S Quintana, J Rabe, B Rahimzadeh, F Rajeevan, M Rayner, D Rayner, NA Raynolds, MK Razuvaev, VN Reagan, J Reid, P Renwick, JA Revadekar, J Rex, M Richter-Menge, J Rivera, IL Robinson, DA Rodell, M Roderick, ML Romanovsky, VE Ronchail, J Rosenlof, KH Rudels, B Sabine, CL Sanchez-Lugo, A Santee, ML Sawaengphokhai, P Sayouri, A Scambos, TA Schauer, U Schemm, J Schmid, C Schreck, C Semiletov, I Send, U Sensoy, S Shakhova, N Sharp, M Shiklomanov, NI Shimada, K Shin, J Siegel, DA Simmons, A Skansi, M Smith, TM Sokolov, V Spence, J Srivastava, AK Stackhouse, PW Stammerjohn, S Steele, M Steffen, K Steinbrecht, W Stephenson, T Stolarski, RS Sweet, W Takahashi, T Taylor, MA Tedesco, M Thepaut, JN Thiaw, WM Thompson, P Thorne, PW Timmermans, ML Tobin, S Toole, J Trachte, K Trewin, BC Trigo, RM Trotman, A Tucker, CJ Ulupinar, Y Van de Wal, RSW van der Werf, GR Vautard, R Votaw, G Wagner, WW Wahr, J Walker, DA Walsh, J Wang, CZ Wang, JH Wang, L Wang, MH Wang, SH Wanninkhof, R Weaver, S Weber, M Weingartner, T Weller, RA Wentz, F Whitewood, R Wilber, AC Willett, KM Williams, W Willis, JK Wilson, RC Wolken, G Wong, TM Woodgate, R Wovrosh, AJ Xue, Y Yamada, R Yamamoto-Kawai, M Yoder, JA Yu, LS Yueh, S Zhang, LY Zhang, PQ Zhao, L Zhou, XJ Zimmermann, S Zubair, L AF Achberger, C. Ackerman, S. A. Ahmed, Farid H. Albanil-Encarnacion, Adelina Alfaro, E. J. Alves, L. M. Allan, Rob Amador, Jorge A. Ambenje, Peter Antoine, M. D. Antonov, John Arevalo, Juan Arndt, Derek S. Ashik, I. Atheru, Zachary Baccini, Alessandro Baez, Julian Banzon, Viva Baringer, Molly O. Barreira, Sandra Barriopedro, D. E. Bates, J. J. Becker, Andreas Behrenfeld, Michael J. Bell, Gerald D. Benedetti, Angela Bernhard, Germar Berrisford, Paul Berry, David I. Beszczynska-Moeller, A. Bhatt, U. S. Bidegain, Mario Bieniek, P. Birkett, Charon Bissolli, Peter Blake, Eric S. Blunden, Jessica Boudet-Rouco, Dagne Box, Jason E. Boyer, Tim Braathen, Geir O. Brackenridge, G. Robert Brohan, Philip Bromwich, David H. Brown, Laura Brown, R. Bruhwiler, Lori Bulygina, O. N. Burrows, John Calderon, Blanca Camargo, Suzana J. Cappellen, John Carmack, E. Carrasco, Gualberto Chambers, Don P. Christiansen, Hanne H. Christy, John Chung, D. Ciais, P. Coehlo, Caio A. S. Colwell, Steve Comiso, J. Cretaux, Jean-Francois Crouch, Jake Cunningham, Stuart A. De Jeu, Richard A. M. Demircan, M. Derksen, C. Diamond, Howard J. Dlugokencky, Ed J. Dohan, Kathleen Dolman, A. Johannes Dorigo, Wouter A. Drozdov, D. S. Duguay, Claude Dutton, Ellsworth Dutton, Geoff S. Elkins, James W. Epstein, H. E. Famiglietti, James S. Fanton d'Andon, Odile Hembise Feely, Richard A. Fekete, Balazs M. Fenimore, Chris Fernandez-Prieto, D. Fields, Erik Fioletov, Vitali Fogt, Ryan L. Folland, Chris Foster, Michael J. Frajka-Williams, Eleanor Franz, Bryan A. Frey, Karen Frith, Stacey H. Frolov, I. Frost, G. V. Ganter, Catherine Garzoli, Silvia Gitau, Wilson Gleason, Karin L. Gobron, Nadine Goldenberg, Stanley B. Goni, Gustavo Gonzalez-Garcia, Idelmis Gonzalez-Rodriguez, Nivaldo Good, Simon A. Goryl, Philippe Gottschalck, Jonathan Gouveia, C. M. Gregg, Margarita C. Griffiths, Georgina M. Grigoryan, Valentina Grooss, Jens-Uwe Guard, Chip Guglielmin, Mauro Hall, Bradley D. Halpert, Michael S. Heidinger, Andrew K. Heikkila, Anu Heim, Richard R., Jr. Hennon, Paula A. Hidalgo, Hugo G. Hilburn, Kyle Ho, Shu-peng Hobbs, Will R. Holgate, Simon Hook, Simon J. Hovsepyan, Anahit Hu, Zeng-Zhen Hugony, Sebastien Hurst, Dale F. Ingvaldsen, R. Itoh, M. Jaimes, Ena Jeffries, Martin Johns, William E. Johnsen, Bjorn Johnson, Bryan Johnson, Gregory C. Jones, L. T. Jumaux, Guillaume Kabidi, Khadija Kaiser, Johannes W. Kang, Kyun-Kuk Kanzow, Torsten O. Kao, Hsun-Ying Keller, Linda M. Kendon, Mike Kennedy, John J. Kervankiran, Sefer Key, J. Khatiwala, Samar Kholodov, A. L. Khoshkam, M. Kikuchi, T. Kimberlain, Todd B. King, Darren Knaff, John A. Korshunova, Natalia N. Koskela, Tapani Kratz, David P. Krishfield, R. Kruger, Andries Kruk, Michael C. Kumar, Arun Lagerloef, Gary Lakkala, Kaisa Lammers, Richard B. Lander, Mark A. Landsea, Chris W. Lankhorst, Matthias Lapinel-Pedroso, Braulio Lazzara, Matthew A. LeDuc, Sharon Lefale, Penehuro Leon, Gloria Leon-Lee, Antonia Leuliette, Eric Levitus, Syndney L'Heureux, Michelle Lin, I. I. Liu, Hongxing Liu, Yanju Liu, Yi Lobato-Sanchez, Rene Locarnini, Ricardo Loeb, Norman G. Loeng, H. Long, Craig S. Lorrey, Andrew M. Lumpkin, Rick Myhre, Cathrine Lund Luo, Jing-Jia Lyman, John M. MacCallum, Stuart Macdonald, Alison M. Maddux, Brent C. Manney, Gloria Marchenko, S. S. Marengo, Jose A. Maritorena, Stephane Marotzke, Jochem Marra, John J. Martinez-Sanchez, Odayls Maslanik, J. Massom, Robert A. Mathis, Jeremy T. McBride, Charlotte McClain, Charles R. McGrath, Daniel McGree, Simon McLaughlin, F. McVicar, Tim R. Mears, Carl Meier, W. Meinen, Christopher S. Menendez, Melisa Merchant, Chris Merrifield, Mark A. Miller, Laury Mitchum, Gary T. Montzka, Stephen A. Moore, Sue Mora, Natalie P. Morcrette, Jean-Jacques Mote, Thomas Muhle, Jens Mullan, A. Brett Muller, Rolf Myhre, Cathrine Nash, Eric R. Nerem, R. Steven Newlin, Michele L. Newman, Paul A. Ngari, Arona Nishino, S. Njau, Lenoard N. Noetzli, Jeannette Oberman, N. G. Obregon, Andre Ogallo, Laban Oludhe, Christopher Overland, J. Oyunjargal, Lamjav Parinussa, R. M. Park, Geun-Ha Parker, David E. Pasch, Richard J. Pascual-Ramirez, Reynaldo Pelto, Mauri S. Penalba, Olga Perez-Suarez, Ramon Perovich, D. Pezza, Alexandre B. Phillips, Dave Pickart, R. Pinty, Bernard Pinzon, J. Pitts, Michael C. Pour, Homa Kheyrollah Prior, John Privette, Jeff L. Proshutinsky, A. Quegan, Shaun Quintana, Juan Rabe, B. Rahimzadeh, Fatemeh Rajeevan, M. Rayner, Darren Rayner, Nick A. Raynolds, M. K. Razuvaev, Vyacheslav N. Reagan, James Reid, Phillip Renwick, James A. Revadekar, J. Rex, Markus Richter-Menge, J. Rivera, Ingrid L. Robinson, David A. Rodell, Matthew Roderick, Michael L. Romanovsky, Vladimir E. Ronchail, Josyane Rosenlof, Karen H. Rudels, B. Sabine, Christopher L. Sanchez-Lugo, Ahira Santee, Michelle L. Sawaengphokhai, P. Sayouri, Amal Scambos, Ted A. Schauer, U. Schemm, Jae Schmid, Claudia Schreck, Carl Semiletov, Igor Send, Uwe Sensoy, Serhat Shakhova, Natalia Sharp, M. Shiklomanov, Nicolai I. Shimada, K. Shin, J. Siegel, David A. Simmons, Adrian Skansi, Maria Smith, Thomas M. Sokolov, V. Spence, Jacqueline Srivastava, A. K. Stackhouse, Paul W., Jr. Stammerjohn, Sharon Steele, M. Steffen, Konrad Steinbrecht, Wolfgang Stephenson, Tannecia Stolarski, Richard S. Sweet, William Takahashi, Taro Taylor, Michael A. Tedesco, Marco Thepaut, Jean-Noel Thiaw, Wassila M. Thompson, Philip Thorne, Peter W. Timmermans, M. L. Tobin, Skie Toole, J. Trachte, Katja Trewin, Blair C. Trigo, Ricardo M. Trotman, Adrian Tucker, C. J. Ulupinar, Yusuf Van de Wal, Roderik S. W. van der Werf, G. R. Vautard, Robert Votaw, Gary Wagner, Wolfgang W. Wahr, John Walker, D. A. Walsh, J. Wang, Chunzai Wang, Junhong Wang, Lei Wang, Menghua Wang, Sheng-Hung Wanninkhof, Rik Weaver, Scott Weber, Mark Weingartner, T. Weller, Robert A. Wentz, Frank Whitewood, Robert Wilber, Anne C. Willett, Kate M. Williams, W. Willis, Joshua K. Wilson, R. Chris Wolken, G. Wong, Takmeng Woodgate, R. Wovrosh, Alex J. Xue, Yan Yamada, Ryuji Yamamoto-Kawai, M. Yoder, James A. Yu, Lisan Yueh, Simon Zhang, Liangying Zhang, Peiqun Zhao, Lin Zhou, Xinjia Zimmerman, S. Zubair, Lafeer TI STATE OF THE CLIMATE IN 2011 Special Supplement to the Bulletin of the American Meteorological Society Vol. 93, No. 7, July 2012 SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID SEA-SURFACE-TEMPERATURE; INTERNATIONAL POLAR YEAR; NORTH-ATLANTIC OSCILLATION; MADDEN-JULIAN OSCILLATION; MERIDIONAL HEAT-TRANSPORT; RESOLUTION IMAGING SPECTRORADIOMETER; OUTGOING LONGWAVE RADIATION; BAND MICROWAVE OBSERVATIONS; NINO SOUTHERN-OSCILLATION; FLORIDA CURRENT TRANSPORT AB Large-scale climate patterns influenced temperature and weather patterns around the globe in 2011. In particular, a moderate-to-strong La Nina at the beginning of the year dissipated during boreal spring but reemerged during fall. The phenomenon contributed to historical droughts in East Africa, the southern United States, and northern Mexico, as well the wettest two-year period (2010-11) on record for Australia, particularly remarkable as this follows a decade-long dry period. Precipitation patterns in South America were also influenced by La Nina. Heavy rain in Rio de Janeiro in January triggered the country's worst floods and landslides in Brazil's history. The 2011 combined average temperature across global land and ocean surfaces was the coolest since 2008, but was also among the 15 warmest years on record and above the 1981-2010 average. The global sea surface temperature cooled by 0.1 degrees C from 2010 to 2011, associated with cooling influences of La Nina. Global integrals of upper ocean heat content for 2011 were higher than for all prior years, demonstrating the Earth's dominant role of the oceans in the Earth's energy budget. In the upper atmosphere, tropical stratospheric temperatures were anomalously warm, while polar temperatures were anomalously cold. This led to large springtime stratospheric ozone reductions in polar latitudes in both hemispheres. Ozone concentrations in the Arctic stratosphere during March were the lowest for that period since satellite records began in 1979. An extensive, deep, and persistent ozone hole over the Antarctic in September indicates that the recovery to pre-1980 conditions is proceeding very slowly. Atmospheric carbon dioxide concentrations increased by 2.10 ppm in 2011, and exceeded 390 ppm for the first time since instrumental records began. Other greenhouse gases also continued to rise in concentration and the combined effect now represents a 30% increase in radiative forcing over a 1990 baseline. Most ozone depleting substances continued to fall. The global net ocean carbon dioxide uptake for the 2010 transition period from El Nino to La Nina, the most recent period for which analyzed data are available, was estimated to be 1.30 Pg C yr(-1), almost 12% below the 29-year long-term average. Relative to the long-term trend, global sea level dropped noticeably in mid-2010 and reached a local minimum in 2011. The drop has been linked to the La Nina conditions that prevailed throughout much of 2010-11. Global sea level increased sharply during the second half of 2011. Global tropical cyclone activity during 2011 was well-below average, with a total of 74 storms compared with the 1981-2010 average of 89. Similar to 2010, the North Atlantic was the only basin that experienced above-normal activity. For the first year since the widespread introduction of the Dvorak intensity-estimation method in the 1980s, only three tropical cyclones reached Category 5 intensity level-all in the Northwest Pacific basin. The Arctic continued to warm at about twice the rate compared with lower latitudes. Below-normal summer snowfall, a decreasing trend in surface albedo, and above-average surface and upper air temperatures resulted in a continued pattern of extreme surface melting, and net snow and ice loss on the Greenland ice sheet. Warmer-than-normal temperatures over the Eurasian Arctic in spring resulted in a new record-low June snow cover extent and spring snow cover duration in this region. In the Canadian Arctic, the mass loss from glaciers and ice caps was the greatest since GRACE measurements began in 2002, continuing a negative trend that began in 1987. New record high temperatures occurred at 20 m below the land surface at all permafrost observatories on the North Slope of Alaska, where measurements began in the late 1970s. Arctic sea ice extent in September 2011 was the second-lowest on record, while the extent of old ice (four and five years) reached a new record minimum that was just 19% of normal. On the opposite pole, austral winter and spring temperatures were more than 3 degrees C above normal over much of the Antarctic continent. However, winter temperatures were below normal in the northern Antarctic Peninsula, which continued the downward trend there during the last 15 years. In summer, an all-time record high temperature of -12.3 degrees C was set at the South Pole station on 25 December, exceeding the previous record by more than a full degree. Antarctic sea ice extent anomalies increased steadily through much of the year, from briefly setting a record low in April, to well above average in December. 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Amer. Meteorol. Soc. PD JUL PY 2012 VL 93 IS 7 SU S BP S1 EP S263 DI 10.1175/2012BAMSStateoftheClimate.1 PG 263 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 979GT UT WOS:000306806200001 ER PT J AU Shah, R Garrison, JL Grant, MS AF Shah, Rashmi Garrison, James L. Grant, Michael S. TI Demonstration of Bistatic Radar for Ocean Remote Sensing Using Communication Satellite Signals SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Ambiguity function; bistatic radar; oceanography; remote sensing; satellite communications ID SCATTERED GPS SIGNALS; SURFACE; SYSTEM; MODEL AB Remote sensing of ocean roughness using reflected signals from digital communication satellites is demonstrated in an airborne experiment. Transmitted data are approximated as an infinitely long sequence of random bits, which is experimentally a hypothesis confirmed for the S-band XM radio signal. On July 2, 2010, a signal recorder was flown at an altitude of 3.17 km off the coast of Virginia, collecting ocean-reflected signals from both geostationary satellites identified as "Rhythm" and "Blues," which were broadcasting the XM radio signal. Direct and reflected signals from the same channel were cross-correlated, producing a waveform that agreed well with a model generated at the 7.5-m/s wind speed reported from the Chesapeake Lighthouse. Adjusting this model to fit the experimental data produced an optimal estimate of 6 m/s. A Monte Carlo approach predicted errors of 0.5% from the simulated reflected XM radio signals and 2%-10% from simulated reflected Global Navigation Satellite System (GNSS-R) signals. This improvement was attributed to the higher (similar to 30 dB) power in the XM radio signal. The availability of communication satellite transmissions, in all frequency bands used for remote sensing, opens the possibility of using signals of opportunity as low-cost alternatives to radiometry or scatterometry. C1 [Shah, Rashmi; Garrison, James L.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Grant, Michael S.] NASA, Langley Res Ctr, Hampton, VA 23666 USA. RP Shah, R (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. EM shah11@purdue.edu FU NASA Langley Research Center [NNX09AH13G, NNX10AE43G] FX This work was supported by the NASA Langley Research Center under Grant NNX09AH13G and Grant NNX10AE43G. NR 15 TC 10 Z9 10 U1 2 U2 23 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 JUL PY 2012 VL 9 IS 4 BP 619 EP 623 DI 10.1109/LGRS.2011.2177061 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 034YW UT WOS:000310909800017 ER PT J AU Thompson, DR Johnson, W Kremens, R AF Thompson, David R. Johnson, William Kremens, Robert TI Multiple-Frame Subpixel Wildfire Tracking SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Computer vision; pattern recognition; smart cameras; thermal imagery; wildfire detection ID ACTIVE FIRE DETECTION; ALGORITHMS; ASTER; MODIS; VALIDATION; SATELLITE; AMERICA; NORTH AB We present a method to improve subpixel signal detection in airborne or orbital image sequences. The proposed technique recognizes stable interest point features in multiple overlapping frames. It estimates motion between consecutive frames and tracks candidate detections over time. The final detection decision combines signal strengths from multiple views to improve sensitivity. The algorithm is computationally tractable for real-time use on autonomous robotic platforms and spacecraft. Additionally, the interest points enable image-relative localization, obviating the need to transmit the entire image and reducing transmission bandwidth requirements by one or more orders of magnitude. This permits higher acquisition rates and potentially improved coverage for remote monitoring. Ground-based systems can reconstruct absolute positions from landmarks without measurements of sensor pose. We demonstrate the algorithm using airborne 4-mu m imagery from multiple overpasses of a controlled wildfire. C1 [Thompson, David R.; Johnson, William] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kremens, Robert] Rochester Inst Technol, Rochester, NY 14623 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; william.r.johnson@jpl.nasa.gov; kremens@cis.rit.edu FU National Aeronautics and Space Administration Jet Propulsion Laboratory Innovative Spontaneous Concept grant; Rochester Institute of Technology Wildfire Airborne Sensor Program team FX Manuscript received April 5, 2011; revised July 22, 2011; accepted November 7, 2011. Date of publication December 30, 2011; date of current version May 7, 2012. This work was supported by a National Aeronautics and Space Administration Jet Propulsion Laboratory Innovative Spontaneous Concept grant.; This work utilized the VLFeat toolbox [14]. The authors would like to thank R. Staehle and M. Burl for their ideas and counsel and the Rochester Institute of Technology Wildfire Airborne Sensor Program team for their support. Finally, the authors would also like to thank M. Chahine. NR 22 TC 1 Z9 1 U1 0 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JUL PY 2012 VL 9 IS 4 BP 639 EP 643 DI 10.1109/LGRS.2011.2177240 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 034YW UT WOS:000310909800021 ER PT J AU Khan, SI Hong, Y Vergara, HJ Gourley, JJ Brakenridge, GR De Groeve, T Flamig, ZL Policelli, F Yong, B AF Khan, Sadiq I. Hong, Yang Vergara, Humberto J. Gourley, Jonathan J. Brakenridge, G. Robert De Groeve, Tom Flamig, Zachary L. Policelli, Frederick Yong, Bin TI Microwave Satellite Data for Hydrologic Modeling in Ungauged Basins SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Digital elevation models (DEMS); distributed hydrologic modeling; floods; passive microwave sensors; satellite remote sensing ID OKAVANGO DELTA; SOIL-MOISTURE; RAINFALL DATA; FLOOD; RIVER; PREDICTION; ALTIMETRY; BOTSWANA; GIS AB An innovative flood-prediction framework is developed using Tropical Rainfall Measuring Mission precipitation forcing and a proxy for river discharge from the Advanced Microwave Scanning Radiometer for Earth Observing System (AMSR-E) onboard the National Aeronautics and Space Administration's Aqua satellite. The AMSR-E-detected water surface signal was correlated with in situ measurements of streamflow in the Okavango Basin in Southern Africa as indicated by a Pearson correlation coefficient of 0.90. A distributed hydrologic model, with structural data sets derived from remote-sensing data, was calibrated to yield simulations matching the flood frequencies from the AMSR-E-detected water surface signal. Model performance during a validation period yielded a Nash-Sutcliffe efficiency of 0.84. We concluded that remote-sensing data from microwave sensors could be used to supplement stream gauges in large sparsely gauged or ungauged basins to calibrate hydrologic models. Given the global availability of all required data sets, this approach can be potentially expanded to improve flood monitoring and prediction in sparsely gauged basins throughout the world. C1 [Khan, Sadiq I.; Hong, Yang; Vergara, Humberto J.] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Khan, Sadiq I.; Hong, Yang; Vergara, Humberto J.; Flamig, Zachary L.] Univ Oklahoma, Atmospher Radar Res Ctr, Norman, OK 73072 USA. [Gourley, Jonathan J.; Flamig, Zachary L.] NOAA, Natl Severe Storms Lab, Natl Weather Ctr, Norman, OK 73072 USA. [Brakenridge, G. Robert] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [De Groeve, Tom] Commiss European Communities, Inst Environm, I-21020 Ispra, Italy. [Policelli, Frederick] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yong, Bin] Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, Nanjing 210098, Jiangsu, Peoples R China. RP Khan, SI (reprint author), Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. EM sadiq@ou.edu; yanghong@ou.edu; humber@ou.edu; Jj.Gourley@noaa.gov; robert.brakenridge@Colorado.edu; tom.de-groeve@jrc.it; Zac.Flamig@noaa.gov; frederick.s.policelli@nasa.gov; binyong@ou.edu RI Hong, Yang/D-5132-2009; Khan, Sadiq/B-8209-2012; Yong, Bin/C-2257-2014; Gourley, Jonathan/C-7929-2016 OI Hong, Yang/0000-0001-8720-242X; Yong, Bin/0000-0003-1466-2091; Gourley, Jonathan/0000-0001-7363-3755 FU National Aeronautics and Space Administration (NASA) Headquarters under the NASA Earth Science Fellowship Program [NNX08AX63H] FX Manuscript received April 8, 2011; revised September 19, 2011 and November 2, 2011; accepted November 19, 2011. Date of publication January 23, 2012; date of current version May 7, 2012. This work was supported by the National Aeronautics and Space Administration (NASA) Headquarters under the NASA Earth Science Fellowship Program under Grant NNX08AX63H. NR 37 TC 19 Z9 19 U1 1 U2 30 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 JUL PY 2012 VL 9 IS 4 BP 663 EP 667 DI 10.1109/LGRS.2011.2177807 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 034YW UT WOS:000310909800026 ER PT J AU England, TD Diestelhorst, RM Kenyon, EW Cressler, JD Ramachandran, V Alles, M Reed, R Berger, R Garbos, R Blalock, B Mantooth, A Barlow, M Dai, F Johnson, W Ellis, C Holmes, J Webber, C McCluskey, P Mojarradi, M Peltz, L Frampton, R Eckert, C AF England, T. D. Diestelhorst, R. M. Kenyon, E. W. Cressler, J. D. Ramachandran, V. Alles, M. Reed, R. Berger, R. Garbos, R. Blalock, B. Mantooth, A. Barlow, M. Dai, F. Johnson, W. Ellis, C. Holmes, J. Webber, C. McCluskey, P. Mojarradi, M. Peltz, L. Frampton, R. Eckert, C. TI A new approach to designing electronic systems for operation in extreme environments: Part II - The SiGe remote electronics unit SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE LA English DT Article ID BASE BIPOLAR TECHNOLOGY; 77-K APPLICATIONS; PROFILE DESIGN; TEMPERATURE; OPTIMIZATION; TRANSISTORS C1 [England, T. D.; Diestelhorst, R. M.; Kenyon, E. W.; Cressler, J. D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Ramachandran, V.; Alles, M.; Reed, R.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA. [Berger, R.; Garbos, R.] BAE Syst, Manassas, VA 20110 USA. [Blalock, B.] Univ Tennessee, Dept Elect Engn & Comp Sci, Knoxville, TN 37996 USA. [Mantooth, A.; Barlow, M.] Univ Arkansas, Dept Elect Engn, Fayetteville, AR 72701 USA. [Dai, F.; Johnson, W.; Ellis, C.] Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. [Holmes, J.; Webber, C.] Lynguent Inc, Fayetteville, AR 72701 USA. [McCluskey, P.] Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA. [Mojarradi, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Peltz, L.; Frampton, R.] Boeing Phantom Works, Seal Beach, CA 90740 USA. [Eckert, C.] Georgia Tech Res Inst, Atlanta, GA 30332 USA. RP England, TD (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, 777 Atlantic Dr NW, Atlanta, GA 30332 USA. RI McCluskey, Patrick/H-6035-2013 FU NASA ETDP [NNL06AA29C] FX This work was supported by NASA ETDP under Contract NNL06AA29C. We are grateful for the support of A. Keys, M. Watson, D. Frazier, M. Beatty, D. Hope and C. Moore of NASA, E. Kolawa of JPL, and A. Joseph, T. Lamothe, and the IBM SiGe development team. NR 25 TC 8 Z9 8 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-8985 J9 IEEE AERO EL SYS MAG JI IEEE Aerosp. Electron. Syst. Mag. PD JUL PY 2012 VL 27 IS 7 BP 29 EP 41 DI 10.1109/MAES.2012.6328839 PG 13 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA 025AI UT WOS:000310154200004 ER PT J AU Sawamura, P Vernier, JP Barnes, JE Berkoff, TA Welton, EJ Alados-Arboledas, L Navas-Guzman, F Pappalardo, G Mona, L Madonna, F Lange, D Sicard, M Godin-Beekmann, S Payen, G Wang, Z Hu, S Tripathi, SN Cordoba-Jabonero, C Hoff, RM AF Sawamura, P. Vernier, J. P. Barnes, J. E. Berkoff, T. A. Welton, E. J. Alados-Arboledas, L. Navas-Guzman, F. Pappalardo, G. Mona, L. Madonna, F. Lange, D. Sicard, M. Godin-Beekmann, S. Payen, G. Wang, Z. Hu, S. Tripathi, S. N. Cordoba-Jabonero, C. Hoff, R. M. TI Stratospheric AOD after the 2011 eruption of Nabro volcano measured by lidars over the Northern Hemisphere SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE Nabro volcano; stratospheric AOD; lidar network ID ASIAN MONSOON TRANSPORT; RAMAN LIDAR; EYJAFJALLAJOKULL ERUPTION; AEROSOL LAYER; DISPERSION; POLLUTION; NETWORK; CLIMATE; EUROPE; CLOUD AB Nabro volcano (13.37 degrees N, 41.70 degrees E) in Eritrea erupted on 13 June 2011 generating a layer of sulfate aerosols that persisted in the stratosphere for months. For the first time we report on ground-based lidar observations of the same event from every continent in the Northern Hemisphere, taking advantage of the synergy between global lidar networks such as EARLINET, MPLNET and NDACC with independent lidar groups and satellite CALIPSO to track the evolution of the stratospheric aerosol layer in various parts of the globe. The globally averaged aerosol optical depth (AOD) due to the stratospheric volcanic aerosol layers was of the order of 0.018 +/- 0.009 at 532 nm, ranging from 0.003 to 0.04. Compared to the total column AOD from the available collocated AERONET stations, the stratospheric contribution varied from 2% to 23% at 532 nm. C1 [Sawamura, P.; Hoff, R. M.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Vernier, J. P.] NASA, Langley Res Ctr, Hampton, VA 23666 USA. [Barnes, J. E.] NOAA, ESRL, Mauna Loa Observ, Hilo, HI 96720 USA. [Berkoff, T. A.; Hoff, R. M.] Joint Ctr Earth Syst Technol, Baltimore, MD USA. [Welton, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Alados-Arboledas, L.; Navas-Guzman, F.] Junta de Andalucia Univ Granada, Ctr Andaluz Medio Ambiente, Granada 18071, Spain. [Pappalardo, G.; Mona, L.; Madonna, F.] CNR, IMAA, I-85050 Potenza, Italy. [Lange, D.; Sicard, M.] Univ Politecn Cataluna, Remote Sensing Lab, E-08034 Barcelona, Spain. [Lange, D.; Sicard, M.] UPC, Inst Estudis Espacials Catalunya, Barcelona, Spain. [Godin-Beekmann, S.; Payen, G.] Univ Paris 06, Lab Atmospheres, CNRS, F-75252 Paris 05, France. [Wang, Z.; Hu, S.] Chinese Acad Sci, Key Lab Atmospher Composit & Opt Radiat, Anhui Inst Opt & Fine Mech, Hefei 230031, Anhui, Peoples R China. [Tripathi, S. N.] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. [Tripathi, S. N.] Indian Inst Technol, Ctr Environm Sci & Engn, Kanpur 208016, Uttar Pradesh, India. [Cordoba-Jabonero, C.] Inst Nacl Tecn Aerospacial, Madrid 28850, Spain. RP Sawamura, P (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM psawamura@umbc.edu RI Sawamura, Patricia/D-1799-2013; Sicard, Michael/K-9064-2013; Cordoba-Jabonero, Carmen/J-6331-2014; Alados-Arboledas, Lucas/P-5630-2014; Navas Guzman, Francisco/G-5900-2016; Tripathi, Sachchida/J-4840-2016; OI MONA, LUCIA/0000-0003-4157-0838; Sicard, Michael/0000-0001-8287-9693; Cordoba-Jabonero, Carmen/0000-0003-4859-471X; Alados-Arboledas, Lucas/0000-0003-3576-7167; Navas Guzman, Francisco/0000-0002-0905-4385; Lange, Diego/0000-0002-1185-7152 FU NASA; National Key Basic Research Project of China [2007FY110700]; EU; Ministry of Earth Sciences, India; Natural Environment Research Council, UK; CNRS INSU; [NNX10AR38G]; [CGL2010-18782]; [P10-RNM-6299] FX The authors would like to thank Simon Carn from the Department of Geological and Mining Engineering and Sciences at Michigan Tech for preliminary SO2 analysis. The authors would also like to acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model and READY website (www.arl.noaa.gov/ready.php) used in this publication. Lidar work at UMBC was funded by grant NNX10AR38G (DISCOVER-AQ). The NASA Micro-Pulse Lidar Network is funded by the NASA Earth Observing System and Radiation Sciences Program. Lidar work at the Hefei site was funded by the National Key Basic Research Project of China under Grant No. 2007FY110700. Lidar work at Universidad de Granada was funded by grants CGL2010-18782 and P10-RNM-6299. The EARLINET stations are funded by the EU FP7 Project 'ACTRIS'. SNT was supported under the program, Changing Water Cycle funded jointly by Ministry of Earth Sciences, India and Natural Environment Research Council, UK. The OHP lidar measurements are funded by CNRS INSU. NR 48 TC 19 Z9 19 U1 3 U2 39 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD JUL-SEP PY 2012 VL 7 IS 3 AR 034013 DI 10.1088/1748-9326/7/3/034013 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 016YH UT WOS:000309555300014 ER PT J AU Trembanis, AC Forrest, AL Miller, DC Lim, DSS Gemhardt, ML Todd, WL AF Trembanis, Arthur C. Forrest, Alex L. Miller, Douglas C. Lim, Darlene S. S. Gemhardt, Michael L. Todd, William L. TI Multiplatform Ocean Exploration: Insights From the NEEMO Space Analog Mission SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Article DE NASA; Conch Reef; Aquarius Reef Base; AUVs; space analogs ID SPONGE XESTOSPONGIA-MUTA; FLORIDA-KEYS; CORAL-REEFS; CONCH REEF; STRATIGRAPHY; GROWTH AB Since the beginning of space exploration, methods and protocols of exploration have been developed using space analogs on Earth to reduce research costs, develop safe deployment/retrieval protocols, and ready astronauts for hostile environments in less threatening settings. Space analogs are required as much as ever today as astronauts and scientists develop new tools and techniques for exploration, while working to address evolving mission objectives from low-earth orbit to deep-space exploration. This study examines coordinated human and robotic exploration at the Aquarius Underwater Habitat off of the coast of Key Largo, Florida, in support of the NEEMO 15 (NASA Extreme Environment Mission Operations) program. The exploration scheme presented in this work fuses (1) robotic precursor missions as a means of remote sensing data collection; (2) crowdsourcing to process immense amounts of data to identify key targets of interest that might be missed in the tight cycle of mission operations; and (3) human exploration to examine locations directly up close and collect physical samples that require involved sampling techniques. Autonomous underwater vehicles (AUVs) and single-person submersibles, called DeepWorkers (TM), were used as underwater analogs of robotic systems currently being used and human-operated vehicles (HOVs) proposed for use on a Near Earth Asteroid (NEA), the Moon, or Mars. In addition to operational lessons learned for space exploration that are directly applicable to ocean exploration, ocean floor mapping provides new levels of detail of benthic habitat critical for coral reef monitoring and management. Opportunistic (onsite adaptive) data sampling also took place by placing self-recording instrumentation onto each of the DeepWorkers, increasing the collection of scientific information during the submersible missions and contributing to mission planning for optimal and efficient use of expensive assets. C1 [Trembanis, Arthur C.; Miller, Douglas C.] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA. [Forrest, Alex L.] Univ Calif Davis, Tahoe Environm Res Ctr, Davis, CA USA. [Lim, Darlene S. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gemhardt, Michael L.; Todd, William L.] NASA, Explorat Miss & Syst Off, Houston, TX USA. RP Trembanis, AC (reprint author), Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA. EM art@udel.edu RI Forrest, Alexander/C-3765-2014 OI Forrest, Alexander/0000-0002-7853-9765 FU NASA through the NEEMO Project [NNX08AR706, GEOL37213311000] FX The authors would like to thank the crew of the NOAA Aquarius Reef Base with special appreciation to Otto Rutten, Saul Rosser, and Ryan LaPete. Project funding provided by NASA through the NEEMO Project (awards NNX08AR706 and GEOL37213311000). Special thanks also go to the PLRP, which was our initiation into the use of AUVs as analogs for space exploration. Members of the NASA IRG (David Lees, Tamar Cohen, and Matthew Deans) are particularly thanked for developing and providing operational support for xGDS. The authors wish to acknowledge the Integration and Application Network, University of Maryland Center for Environmental Science (http://ian.umces.edu/imagelibrary/), for use of some of the royalty-free vector images of reef flora, fauna, SCUBA diver, and the Aquarius Underwater Habitat. Thanks to Nuytco, Ltd., for providing the graphic of the Deep Worker submersible. Thanks to all those who contributed their time and effort to this project, including Mark Patterson (Virginia Institute of Marine Science), Margarita Marinova and Paul Abell (NASA), Howard Mendlovitz and Chris Martens (University of North Carolina), Allyson Brady (University of Calgary), and Emma Hickerson and G.P. Schmahl (NOAA's Office of National Marine Sanctuaries) for giving feedback on underwater robotics, space exploration, and reef science. Thanks also to Prof. Geoff Schladow for comments and support during this work and Val Schmidt, Nicole Raineault, Hilary Stevens, Bryan Keller, John Gutsche, and Lyle De La Rosa for logistical assistance. Additional project technical support has come from University of New Hampshire Center for Coastal and Ocean Mapping/Joint Hydrographic Center, Teledyne-Gavia, Nuytco Ltd., GeoAcoustics, Quester Tangent, Yellow Spring Instrument, and Chesapeake Technology, Inc. NR 37 TC 0 Z9 0 U1 1 U2 9 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 EI 1948-1209 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD JUL-AUG PY 2012 VL 46 IS 4 BP 7 EP 19 PG 13 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 013VQ UT WOS:000309334400002 ER PT J AU Wulder, MA Masek, JG AF Wulder, Michael A. Masek, Jeffrey G. TI Preface to Landsat Legacy Special Issue: Continuing the Landsat Legacy SO REMOTE SENSING OF ENVIRONMENT LA English DT Editorial Material C1 [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Washington, DC USA. EM mwulder@nrcan.gc.ca RI Masek, Jeffrey/D-7673-2012; Wulder, Michael/J-5597-2016 OI Wulder, Michael/0000-0002-6942-1896 NR 0 TC 3 Z9 4 U1 0 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL PY 2012 VL 122 SI SI BP 1 EP 1 DI 10.1016/j.rse.2012.01.009 PG 1 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 004KM UT WOS:000308680600001 ER PT J AU Wulder, MA Masek, JG Cohen, WB Loveland, TR Woodcock, CE AF Wulder, Michael A. Masek, Jeffrey G. Cohen, Warren B. Loveland, Thomas R. Woodcock, Curtis E. TI Opening the archive: How free data has enabled the science and monitoring promise of Landsat SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat; Archive; Science; Policy; Applications; Monitoring; Mapping ID DATA CONTINUITY MISSION; TIME-SERIES DATA; FOREST DISTURBANCE; SURFACE REFLECTANCE; LANDSCAPE METRICS; THEMATIC MAPPER; WESTERN OREGON; BOREAL FORESTS; SATELLITE DATA; UNITED-STATES AB Landsat occupies a unique position in the constellation of civilian earth observation satellites, with a long and rich scientific and applications heritage. With nearly 40 years of continuous observation - since launch of the first satellite in 1972 - the Landsat program has benefited from insightful technical specification, robust engineering, and the necessary infrastructure for data archive and dissemination. Chiefly, the spatial and spectral resolutions have proven of broad utility and have remained largely stable over the life of the program. The foresighted acquisition and maintenance of a global image archive has proven to be of unmatched value, providing a window into the past and fueling the monitoring and modeling of global land cover and ecological change. In this paper we discuss the evolution of the Landsat program as a global monitoring mission, highlighting in particular the recent change to an open (free) data policy. The new data policy is revolutionizing the use of Landsat data, spurring the creation of robust standard products and new science and applications approaches. Open data access also promotes increased international collaboration to meet the Earth observing needs of the 21st century. Crown Copyright (C) 2012 Published by Elsevier Inc. All rights reserved. C1 [Wulder, Michael A.] Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC V8Z 1M5, Canada. [Masek, Jeffrey G.] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cohen, Warren B.] US Forest Serv, USDA, PNW Res Stn, Corvallis, OR 97331 USA. [Loveland, Thomas R.] US Geol Survey, Earth Observat & Sci EROS Ctr, Sioux Falls, SD 57198 USA. [Woodcock, Curtis E.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. RP Wulder, MA (reprint author), Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, 506 W Burnside Rd, Victoria, BC V8Z 1M5, Canada. EM mwulder@nrcan.gc.ca RI Masek, Jeffrey/D-7673-2012; Trivedi, Kruti/E-7558-2015; Wulder, Michael/J-5597-2016 OI Wulder, Michael/0000-0002-6942-1896 NR 80 TC 203 Z9 207 U1 10 U2 79 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL PY 2012 VL 122 SI SI BP 2 EP 10 DI 10.1016/j.rse.2012.01.010 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 004KM UT WOS:000308680600002 ER PT J AU Irons, JR Dwyer, JL Barsi, JA AF Irons, James R. Dwyer, John L. Barsi, Julia A. TI The next Landsat satellite: The Landsat Data Continuity Mission SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat Data Continuity Mission; Operational Land Imager; Thermal Infrared Sensor; National Aeronautics and Space Administration; Goddard Space Flight Center; United States Geological Survey; Earth Resources Science and Observation Center AB The National Aeronautics and Space Administration (NASA) and the Department of Interior United States Geological Survey (USGS) are developing the successor mission to Landsat 7 that is currently known as the Landsat Data Continuity Mission (LDCM). NASA is responsible for building and launching the LDCM satellite observatory. USGS is building the ground system and will assume responsibility for satellite operations and for collecting, archiving, and distributing data following launch. The observatory will consist of a spacecraft in low-Earth orbit with a two-sensor payload. One sensor, the Operational Land Imager (OLI), will collect image data for nine shortwave spectral bands over a 185 km swath with a 30 m spatial resolution for all bands except a 15 m panchromatic band. The other instrument, the Thermal Infrared Sensor (TIRS), will collect image data for two thermal bands with a 100 m resolution over a 185 km swath. Both sensors offer technical advancements over earlier Landsat instruments. OLI and TIRS will coincidently collect data and the observatory will transmit the data to the ground system where it will be archived, processed to Level 1 data products containing well calibrated and co-registered OLI and TIRS data, and made available for free distribution to the general public. The LDCM development is on schedule for a December 2012 launch. The USGS intends to rename the satellite "Landsat 8" following launch. By either name a successful mission will fulfill a mandate for Landsat data continuity. The mission will extend the almost 40-year Landsat data archive with images sufficiently consistent with data from the earlier missions to allow long-term studies of regional and global land cover change. Published by Elsevier Inc. C1 [Irons, James R.] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dwyer, John L.] US Geol Survey, Earth Resources Observat & Sci EROS Ctr, Sioux Falls, SD 57198 USA. [Barsi, Julia A.] NASA, Sci Syst & Applicat Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Irons, JR (reprint author), NASA, Atmospheres Lab, Goddard Space Flight Ctr, Code 613-0, Greenbelt, MD 20771 USA. EM james.r.irons@nasa.gov; dwyer@usgs.gov; julia.a.barsi@nasa.gov OI Dwyer, John/0000-0002-8281-0896 NR 14 TC 211 Z9 223 U1 8 U2 99 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL PY 2012 VL 122 SI SI BP 11 EP 21 DI 10.1016/j.rse.2011.08.026 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 004KM UT WOS:000308680600003 ER PT J AU Markham, BL Helder, DL AF Markham, Brian L. Helder, Dennis L. TI Forty-year calibrated record of earth-reflected radiance from Landsat: A review SO REMOTE SENSING OF ENVIRONMENT LA English DT Review DE Landsat; Radiometric Calibration; History; MSS; TM; ETM ID THEMATIC MAPPER; RADIOMETRIC CALIBRATION; SENSORS; ETM+; SITES AB Sensors on Landsat satellites have been collecting images of the Earth's surface for nearly 40 years. These images have been invaluable for characterizing and detecting changes in the land cover and land use of the world. Although initially conceived as primarily picture generating sensors, even the early sensors were radiometrically calibrated and spectrally characterized prior to launch and incorporated some capabilities to monitor their radiometric calibration once on orbit. Recently, as the focus of studies has shifted to monitoring Earth surface parameters over significant periods of time, serious attention has been focused toward bringing the data from all these sensors onto a common radiometric scale over this 40-year period. This effort started with the most recent systems and then was extended back in time. Landsat-7 Enhanced Thematic Mapper (ETM)+, the best-characterized sensor of the series prior to launch and once on orbit, and the most stable system to date, was chosen to serve as the reference. The Landsat-7 project was the first of the series to build an image assessment system into its ground system, allowing systematic characterization of its sensors and data. Second, the Landsat-5 Thematic Mapper (TM) (still operating at the time of the Landsat-7 launch and continues to operate) calibration history was reconstructed based on its internal calibrator, vicarious calibrations, pseudo-invariant sites and a tie to Landsat-7 ETM + at the time of the commissioning of Landsat-7. This process was performed in two iterations: the earlier one relied primarily on the TM internal calibrator. When this was found to have some deficiencies, a revised calibration was based more on pseudo-invariant sites, though the internal calibrator was still used to establish the short-term variations in response due to contaminant build up on the cold focal plane. As time progressed, a capability to monitor the Landsat-5 TM was added to the image assessment system. The Landsat-4 TM, which operated from 1982 to 1992, was the third system to which the radiometric scale was extended. The limited and broken use of the Landsat-4 TM made this analysis more difficult. Eight-day separated image pairs from Landsat-5 combined with analysis of pseudo invariant sites established this history. The fourth and most challenging effort was making the Landsat 1-5 Multi-Spectral Scanner (MSS) sensors' data internally radiometrically consistent. This effort was particularly complicated by the age of the MSS data, varying formats and processing levels in the archive, limited datasets, and limited documentation available. Ultimately, pseudo-invariant sites were identified in North America and used for this effort. Note that most of the Landsat MSS archived data had already been calibrated using the MSS internal calibrators, so this processing was embedded in the result The final effort was developing an absolute scale for Landsat MSS similar to what was already established for the "TM" sensors. This was accomplished by using simultaneous data from Landsat-5 MSS and Landsat-5 TM, accounting for spectral differences between the sensors using EO-1 Hyperion data. The recalibrated history of the Landsat data and implications to users are discussed. The key result from this work is a consistently calibrated Landsat data archive that spans nearly 40 years with total uncertainties on the order of 10% or less for most sensors and bands. Published by Elsevier Inc. C1 [Markham, Brian L.] NASA, Biospher Sci Lab, GSFC, Greenbelt, MD 20771 USA. [Helder, Dennis L.] S Dakota State Univ, Coll Engn, Brookings, SD 57007 USA. RP Markham, BL (reprint author), NASA, Biospher Sci Lab, GSFC, Code 618, Greenbelt, MD 20771 USA. EM Brian.L.Markham@nasa.gov; Dennis.Helder@sdstate.edu RI Markham, Brian/M-4842-2013 OI Markham, Brian/0000-0002-9612-8169 NR 27 TC 64 Z9 68 U1 6 U2 51 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL PY 2012 VL 122 SI SI BP 30 EP 40 DI 10.1016/j.rse.2011.06.026 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 004KM UT WOS:000308680600005 ER PT J AU Schott, JR Hook, SJ Barsi, JA Markham, BL Miller, J Padula, FP Raqueno, NG AF Schott, John R. Hook, Simon J. Barsi, Julia A. Markham, Brian L. Miller, Jonathan Padula, Francis P. Raqueno, Nina G. TI Thermal infrared radiometric calibration of the entire Landsat 4, 5, and 7 archive (1982-2010) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Infrared; Radiometric calibration; Landsat; Residual uncertainty ID IN-FLIGHT VALIDATION; LAKE TAHOE; SITE; CA/NV; BAND; USA; TM AB Landsat's continuing record of the thermal state of the earth's surface represents the only long term (1982 to the present) global record with spatial scales appropriate for human scale studies (i.e., tens of meters). Temperature drives many of the physical and biological processes that impact the global and local environment. As our knowledge of, and interest in, the role of temperature on these processes have grown, the value of Landsat data to monitor trends and process has also grown. The value of the Landsat thermal data archive will continue to grow as we develop more effective ways to study the long term processes and trends affecting the planet. However, in order to take proper advantage of the thermal data, we need to be able to convert the data to surface temperatures. A critical step in this process is to have the entire archive completely and consistently calibrated into absolute radiance so that it can be atmospherically compensated to surface leaving radiance and then to surface radiometric temperature. This paper addresses the methods and procedures that have been used to perform the radiometric calibration of the earliest sizable thermal data set in the archive (Landsat 4 data). The completion of this effort along with the updated calibration of the earlier (1985-1999) Landsat 5 data, also reported here, concludes a comprehensive calibration of the Landsat thermal archive of data from 1982 to the present. (C) 2012 Elsevier Inc. All rights reserved. C1 [Schott, John R.; Raqueno, Nina G.] Rochester Inst Technol, Rochester, NY 14623 USA. [Hook, Simon J.] NASA, Jet Prop Lab, CALTECH, Washington, DC USA. [Barsi, Julia A.] NASA, Sci Syst & Applicat Inc, Washington, DC USA. [Markham, Brian L.] NASA, GFSC, Washington, DC USA. RP Schott, JR (reprint author), Rochester Inst Technol, Rochester, NY 14623 USA. EM schott@cis.rit.edu RI Markham, Brian/M-4842-2013 OI Markham, Brian/0000-0002-9612-8169 NR 24 TC 16 Z9 18 U1 1 U2 16 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 JUL PY 2012 VL 122 SI SI BP 41 EP 49 DI 10.1016/j.rse.2011.07.022 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 004KM UT WOS:000308680600006 ER PT J AU Ju, JC Roy, DP Vermote, E Masek, J Kovalskyy, V AF Ju, Junchang Roy, David P. Vermote, Eric Masek, Jeffrey Kovalskyy, Valeriy TI Continental-scale validation of MODIS-based and LEDAPS Landsat ETM plus atmospheric correction methods SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat; MODIS; Atmospheric correction; Web-enabled Landsat Data (WELD); Landsat Ecosystem Disturbance Adaptive Processing System (LEDAPS) ID VEGETATION INDEXES; PART I; AEROSOL; IMAGERY; CALIBRATION; ALGORITHM; SENSORS; TM AB The potential of Landsat data processing to provide systematic continental scale products has been demonstrated by several projects including the NASA Web-enabled Landsat Data (WELD) project. The recent free availability of Landsat data increases the need for robust and efficient atmospheric correction algorithms applicable to large volume Landsat data sets. This paper compares the accuracy of two Landsat atmospheric correction methods: a MODIS-based method and the Landsat Ecosystem Disturbance Adaptive Processing System (LEDAPS) method. Both methods are based on the 6SV radiative transfer code but have different atmospheric characterization approaches. The MODIS-based method uses the MODIS Terra derived dynamic aerosol type, aerosol optical thickness, and water vapor to atmospherically correct ETM+ acquisitions in each coincident orbit. The LEDAPS method uses aerosol characterizations derived independently from each Landsat acquisition and assumes a fixed continental aerosol type and uses ancillary water vapor. Validation results are presented comparing ETM+ atmospherically corrected data generated using these two methods with AERONET corrected ETM+ data for 95 10 km x 10 km 30 m subsets, a total of nearly 8 million 30 m pixels, located across the conterminous United States. The results indicate that the MODIS-based method has better accuracy than the LEDAPS method for the ETM+ red and longer wavelength bands. (C) 2012 Elsevier Inc. All rights reserved. C1 [Ju, Junchang; Roy, David P.; Kovalskyy, Valeriy] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA. [Vermote, Eric] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Masek, Jeffrey] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ju, JC (reprint author), S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA. EM junchang.ju@sdstate.edu RI Masek, Jeffrey/D-7673-2012; Vermote, Eric/K-3733-2012 FU NASA's Terrestrial Ecology Program; NASA [NNX08AL93A] FX The LEDAPS project was funded by NASA's Terrestrial Ecology Program. This Web-enabled Landsat Data (WELD) project is funded by NASA's Making Earth System Data Records for Use in Research Environments (MEaSUREs) program, grant number NNX08AL93A. The U.S. Landsat project management and staff are thanked for provision of the Landsat ETM+ data. The AERONET PIs and their staff are thanked for establishing and maintaining the CONUS AERONET sites used in this study. NR 28 TC 51 Z9 54 U1 4 U2 40 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL PY 2012 VL 122 SI SI BP 175 EP 184 DI 10.1016/j.rse.2011.12.025 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 004KM UT WOS:000308680600016 ER PT J AU Ganguly, S Nemani, RR Zhang, G Hashimoto, H Milesi, C Michaelis, A Wang, WL Votava, P Samanta, A Melton, F Dungan, JL Vermote, E Gao, F Knyazikhin, Y Myneni, RB AF Ganguly, Sangram Nemani, Ramakrishna R. Zhang, Gong Hashimoto, Hirofumi Milesi, Cristina Michaelis, Andrew Wang, Weile Votava, Petr Samanta, Arindam Melton, Forrest Dungan, Jennifer L. Vermote, Eric Gao, Feng Knyazikhin, Yuri Myneni, Ranga B. TI Generating global Leaf Area Index from Landsat: Algorithm formulation and demonstration SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Leaf Area Index (LAI); Landsat; Global Land Survey (GLS); Canopy spectral invariants ID PHOTOSYNTHETICALLY ACTIVE RADIATION; FOREST REFLECTANCE MODEL; SYSTEM DATA RECORD; CONIFEROUS FOREST; LAI PRODUCTS; UNDERSTORY VEGETATION; SPECTRAL INVARIANTS; SURFACE REFLECTANCE; BOREAL FORESTS; NORTH-AMERICA AB This paper summarizes the implementation of a physically based algorithm for the retrieval of vegetation green Leaf Area Index (LAI) from Landsat surface reflectance data. The algorithm is based on the canopy spectral invariants theory and provides a computationally efficient way of parameterizing the Bidirectional Reflectance Factor (BRF) as a function of spatial resolution and wavelength. LAI retrievals from the application of this algorithm to aggregated Landsat surface reflectances are consistent with those of MODIS for homogeneous sites represented by different herbaceous and forest cover types. Example results illustrating the physics and performance of the algorithm suggest three key factors that influence the LAI retrieval process: 1) the atmospheric correction procedures to estimate surface reflectances; 2) the proximity of Landsat-observed surface reflectance and corresponding reflectances as characterized by the model simulation: and 3) the quality of the input land cover type in accurately delineating pure vegetated components as opposed to mixed pixels. Accounting for these factors, a pilot implementation of the LAI retrieval algorithm was demonstrated for the state of California utilizing the Global Land Survey (GLS) 2005 Landsat data archive. In a separate exercise, the performance of the LAI algorithm over California was evaluated by using the short-wave infrared band in addition to the red and near-infrared bands. Results show that the algorithm, while ingesting the short-wave infrared band, has the ability to delineate open canopies with understory effects and may provide useful information compared to a more traditional two-band retrieval. Future research will involve implementation of this algorithm at continental scales and a validation exercise will be performed in evaluating the accuracy of the 30-m LAI products at several field sites. (C) 2012 Elsevier Inc. All rights reserved. C1 [Ganguly, Sangram] NASA, BAERI, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nemani, Ramakrishna R.; Dungan, Jennifer L.] NASA, Biospher Sci Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zhang, Gong] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. [Hashimoto, Hirofumi; Milesi, Cristina; Michaelis, Andrew; Wang, Weile; Votava, Petr; Melton, Forrest] Calif State Univ Monterey Bay, Dept Sci & Environm Policy, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Samanta, Arindam] Atmospher & Environm Res AER Inc, Lexington, MA 02421 USA. [Vermote, Eric] Univ Maryland, Dept Geog, College Pk, MD 20771 USA. [Gao, Feng] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Knyazikhin, Yuri; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. RP Ganguly, S (reprint author), NASA, BAERI, Ames Res Ctr, MS 242-4, Moffett Field, CA 94035 USA. EM sangramganguly@gmail.com RI Vermote, Eric/K-3733-2012; ganguly, sangram/B-5108-2010; Myneni, Ranga/F-5129-2012; Dungan, Jennifer/G-9921-2016 OI Dungan, Jennifer/0000-0002-4863-1616 FU NASA FX We acknowledge funding from Earth Science and Advanced Information Systems Technology programs at NASA. We would also like to extend our thanks to all the anonymous reviewers for their constructive comments, which did help us to improve and strengthen the paper. This research was performed using NASA Earth Exchange. NEX combines state-of-the-art supercomputing, Earth system modeling, remote sensing data from NASA and other agencies, and a scientific social networking platform to deliver a complete work environment in which users can explore and analyze large Earth science data sets, run modeling codes, collaborate on new or existing projects, and share results within and/or among communities. NR 59 TC 41 Z9 45 U1 1 U2 53 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JUL PY 2012 VL 122 SI SI BP 185 EP 202 DI 10.1016/j.rse.2011.10.032 PG 18 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 004KM UT WOS:000308680600017 ER PT J AU Kausinis, S Yee, K Barauskas, R AF Kausinis, Saulius Yee, Karl Barauskas, Rimantas TI Estimation of thermo-elastic damping of vibrations in micro-electro-mechanical systems resonators: finite element modeling SO JOURNAL OF MICRO-NANOLITHOGRAPHY MEMS AND MOEMS LA English DT Article DE MEMS vibrations; thermo-elastic dissipation; quality factor; finite element modeling ID INTERNAL-FRICTION; MEMS RESONATORS AB The authors investigated finite element (FE) analysis of damped modal vibrations in complex geometries of micro-electromechanical (MEM) resonators. Q-factor values were determined by taking the thermo-elastic damping into account. The basic model created is presented as a system of partial differential equations, which describe the elastic and thermal phenomena in the MEM structure. Mathematically the problem is formulated as a complex eigenvalue problem. Modal properties of square-and ring-shaped bulk-mode MEM resonators were investigated by taking into account the layered structure of the MEM system and the influence of the geometry of the clamping zone. The calculations were performed by employing the COMSOL Multiphysics FE software. The solution method was verified by comparing numerically and analytically obtained damped modal properties of a MEM cantilever resonator. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.JMM.11.3.033005] C1 [Kausinis, Saulius] Kaunas Univ Technol, Dept Engn Mech, LT-44029 Kaunas, Lithuania. [Yee, Karl] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barauskas, Rimantas] Kaunas Univ Technol, Dept Syst Anal, LT-51368 Kaunas, Lithuania. RP Kausinis, S (reprint author), Kaunas Univ Technol, Dept Engn Mech, 73 K Donelaicio St, LT-44029 Kaunas, Lithuania. EM saulius.kausinis@ktu.lt FU NATO RTO [LTU-AVT-05/1, LTU-AVT-07/1] FX The authors acknowledge the financial support provided by NATO RTO; Projects LTU-AVT-05/1 and LTU-AVT-07/1. NR 22 TC 1 Z9 1 U1 1 U2 8 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1932-5150 J9 J MICRO-NANOLITH MEM JI J. Micro-Nanolithogr. MEMS MOEMS PD JUL-SEP PY 2012 VL 11 IS 3 AR 033005 DI 10.1117/1.JMM.11.3.033005 PG 11 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Optics SC Engineering; Science & Technology - Other Topics; Materials Science; Optics GA 000OD UT WOS:000308394800018 ER PT J AU Begault, DR AF Begault, Durand R. TI Guidelines for NextGen Auditory Displays SO JOURNAL OF THE AUDIO ENGINEERING SOCIETY LA English DT Article ID SYSTEMS; DESIGN; ALARMS AB The Next-Generation Air Transportation System (NextGen) represents a major reconfiguration of the National Airspace System (NAS) within the United States by the Federal Aviation Administration (FAA) over the coming years. This document reviews auditory display design approaches and requirements for NextGen flight decks and air traffic control workstations. While some aspects of auditory alert design are well understood, the overall design of auditory displays must be considered from the perspective of the totality of auditory input to the listener, including speech, alerting signals, and noise. Recommendations for best practices and future research needs specific to NextGen auditory displays are given. C1 NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. RP Begault, DR (reprint author), NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. EM DurandR.Begault@NASA.gov FU NASA-FAA; NASA FX The assistance of my colleagues at NASA Ames Research Center's Advanced Controls and Displays Laboratory is gratefully acknowledged. Support was received from the NASA-FAA Workstation Integration project as well as from NASA's Integrated Intelligent Flight Deck Project. NR 47 TC 1 Z9 1 U1 0 U2 1 PU AUDIO ENGINEERING SOC PI NEW YORK PA 60 E 42ND ST, NEW YORK, NY 10165-2520 USA SN 1549-4950 J9 J AUDIO ENG SOC JI J. Audio Eng. Soc. PD JUL-AUG PY 2012 VL 60 IS 7-8 BP 519 EP 530 PG 12 WC Acoustics; Engineering, Multidisciplinary SC Acoustics; Engineering GA 005WE UT WOS:000308780000004 ER PT J AU Bengtsson, J Hartmann, M Unterseher, M Vaishampayan, P Abarenkov, K Durso, L Bik, EM Garey, JR Eriksson, KM Nilsson, RH AF Bengtsson, Johan Hartmann, Martin Unterseher, Martin Vaishampayan, Parag Abarenkov, Kessy Durso, Lisa Bik, Elisabeth M. Garey, James R. Eriksson, K. Martin Nilsson, R. Henrik TI Megraft: a software package to graft ribosomal small subunit (16S/18S) fragments onto full-length sequences for accurate species richness and sequencing depth analysis in pyrosequencing-length metagenomes and similar environmental datasets SO RESEARCH IN MICROBIOLOGY LA English DT Article DE Metagenomics; Rarefaction; Species richness analysis; rDNA; 16S; 18S ID RNA GENE-SEQUENCES; DIVERSITY; QUALITY AB Metagenomic libraries represent subsamples of the total DNA found at a study site and offer unprecedented opportunities to study ecological and functional aspects of microbial communities. To examine the depth of a community sequencing effort, rarefaction analysis of the ribosomal small subunit (SSU/16S/18S) gene in the metagenome is usually performed. The fragmentary, non-overlapping nature of SSU sequences in metagenomic libraries poses a problem for this analysis, however. We introduce a software package - Megraft - that grafts SSU fragments onto full-length SSU sequences, accounting for observed and unobserved variability, for accurate assessment of species richness and sequencing depth in metagenomics endeavors. (c) 2012 Institut Pasteur. Published by Elsevier Masson SAS. All rights reserved. C1 [Bengtsson, Johan] Univ Gothenburg, Inst Neurosci & Physiol, Sahlgrenska Acad, S-40530 Gothenburg, Sweden. [Bengtsson, Johan; Eriksson, K. Martin; Nilsson, R. Henrik] Univ Gothenburg, Dept Biol & Environm Sci, S-40530 Gothenburg, Sweden. [Hartmann, Martin] Agroscope Reckenholz Tanikon Res Stn ART, CH-8046 Zurich, Switzerland. [Hartmann, Martin] Swiss Fed Res Inst WSL, CH-8903 Birmensdorf, Switzerland. [Unterseher, Martin] Ernst Moritz Arndt Univ Greifswald, Inst Bot & Landscape Ecol, D-17487 Greifswald, Germany. [Vaishampayan, Parag] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. [Abarenkov, Kessy] Univ Tartu, Nat Hist Museum, EE-51014 Tartu, Estonia. [Durso, Lisa] ARS, USDA, Agroecosyst Management Res Unit, Lincoln, NE 68583 USA. [Bik, Elisabeth M.] Stanford Sch Med, Dept Microbiol & Immunol, Stanford, CA 94305 USA. [Garey, James R.] Univ S Florida, Dept Cell Biol Microbiol & Mol Biol, Tampa, FL 33620 USA. [Nilsson, R. Henrik] Univ Tartu, Inst Ecol & Earth Sci, Dept Bot, EE-50090 Tartu, Estonia. RP Bengtsson, J (reprint author), Univ Gothenburg, Inst Neurosci & Physiol, Sahlgrenska Acad, Medicinaregatan 11,Box 434, S-40530 Gothenburg, Sweden. EM johan@microbiology.se; martin.hartmann@microbiome.ch; martin.unterseher@uni-greifswald.de; Parag.A.Vaishampayan@jpl.nasa.gov; kessy@ut.ee; Lisa.Durso@ars.usda.gov; eliesbik@stanford.edu; garey@usf.edu; martin.eriksson@bioenv.gu.se; henrik.nilsson@bioenv.gu.se RI Bengtsson-Palme, Johan/K-3871-2012; Unterseher, Martin/B-2381-2014; Eriksson, Karl/D-7811-2015; Abarenkov, Kessy/H-9611-2015; Hartmann, Martin/M-9371-2016; Bik, Elisabeth/A-1204-2007; OI Bengtsson-Palme, Johan/0000-0002-6528-3158; Eriksson, Karl/0000-0001-7437-7175; Abarenkov, Kessy/0000-0001-5526-4845; Hartmann, Martin/0000-0001-8069-5284; Bik, Elisabeth/0000-0001-5477-0324; Nilsson, Henrik/0000-0002-8052-0107 NR 29 TC 10 Z9 10 U1 0 U2 21 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0923-2508 J9 RES MICROBIOL JI Res. Microbiol. PD JUL-AUG PY 2012 VL 163 IS 6-7 BP 407 EP 412 DI 10.1016/j.resmic.2012.07.001 PG 6 WC Microbiology SC Microbiology GA 007PU UT WOS:000308901400002 PM 22824070 ER PT J AU Landi, E Bhatia, AK AF Landi, E. Bhatia, A. K. TI Atomic data and spectral line intensities for Ni XV SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID SOLAR SPECTRUM; EMISSION-LINES; WAVELENGTHS; ELEMENTS; NICKEL; IDENTIFICATIONS; ANGSTROMS; STRENGTHS; SEQUENCE; CHIANTI AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Ni XV. We include in the calculations the 9 lowest configurations, corresponding to 126 fine structure levels: 3s(2)3p(2), 3s3p(3), 3s(2)3p3d, 3p(4), 3s3p(2)3d, and 3s(2) 3p4I with I =, s, p, d, f. Collision strengths are calculated at five incident energies for all transitions: 7.8, 18.5, 33.5, 53.5, and 80.2 Ry above the threshold of each transition. An additional energy, very close to the transition threshold, has been added, whose value is between 0.004 and 0.28 Ry depending on the levels involved. Calculations have been carried out using the Flexible Atomic Code and the distorted-wave approximation. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates calculated in the present work, statistical equilibrium equations for level populations are solved at electron densities covering the 10(8)-10(14) cm(-3) range and at an electron temperature of log T-e (K) = 6.4, corresponding to the maximum abundance of Ni XV. Spectral line intensities are calculated, and their diagnostic relevance is discussed. This dataset will be made available in the next version of the CHIANTI database. (C) 2012 Elsevier Inc. All rights reserved. C1 [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Landi, E (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM elandi@umich.edu RI Landi, Enrico/H-4493-2011 FU NASA [NNX10AM17G, NNX11AC20G] FX The work of Enrico Landi is supported by NASA grants NNX10AM17G and NNX11AC20G. Calculations were carried out using Discover computer of the NASA Center for Computation Science. The authors thank the referee for his/her valuable comments that helped them to improve the original manuscript. NR 43 TC 6 Z9 6 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD JUL PY 2012 VL 98 IS 4 BP 862 EP 893 DI 10.1016/j.adt.2012.05.002 PG 32 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA 998WR UT WOS:000308271600013 ER PT J AU Serafy, JE Cooke, SJ Diaz, GA Graves, JE Hall, M Shivji, M Swimmer, Y AF Serafy, Joseph E. Cooke, Steven J. Diaz, Guillermo A. Graves, John E. Hall, Martin Shivji, Mahmood Swimmer, Yonat TI CIRCLE HOOKS IN COMMERCIAL, RECREATIONAL, AND ARTISANAL FISHERIES: RESEARCH STATUS AND NEEDS FOR IMPROVED CONSERVATION AND MANAGEMENT SO BULLETIN OF MARINE SCIENCE LA English DT Article ID PELAGIC LONGLINE FISHERY; SPINY DOGFISH; CATCH RATES; SEA-TURTLES; BY-CATCH; BYCATCH; REDUCE; MORTALITY; MARINE; MARLIN AB The intent of convening the International Symposium on Circle Hooks in Research, Management, and Conservation was to yield a contemporary, science-based assessment of the management and conservation utility of circle hooks in commercial, recreational, and artisanal fisheries around the globe. The symposium objective was to provide a forum for individuals, organizations, and agencies to share relevant research results and perspectives. Based on the presentations, an examination of the literature, and the collective experience and knowledge of the authors, we provide a brief overview of the current status of circle hook research along with a list of research needs, with a particular focus on science that has the potential to inform managers and stakeholders. Progress was made on the definition of a "true circle hook." There was strong recognition that circle hooks represent just one of the tools available to managers for reducing bycatch and release mortality. Also defined was the need for an integrative approach that considers strategies that complement the use of circle hooks. Some of the research needs identified include a greater emphasis on human dimension studies to identify those factors that may impede adoption of circle hook technology by stakeholders and comparative studies of circle hook performance relative to mouth morphology, dentition, and feeding behavior. While the literature on effective use of circle hooks is growing, there remains a number of unanswered questions that will require study before circle hooks are more widely adopted for conservation and management of aquatic living resources. C1 [Serafy, Joseph E.; Diaz, Guillermo A.] NOAA, SE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Miami, FL 33149 USA. [Cooke, Steven J.] Carleton Univ, Dept Biol, Fish Ecol & Conservat Physiol Lab, Ottawa, ON K1S 5B6, Canada. [Graves, John E.] Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, Williamsburg, VA 23062 USA. [Hall, Martin] Interamer Trop Tuna Commiss, La Jolla, CA 92037 USA. [Shivji, Mahmood] Nova SE Univ, Guy Harvey Res Inst, Dania, FL 33004 USA. [Swimmer, Yonat] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Long Beach, CA 92037 USA. RP Serafy, JE (reprint author), NOAA, SE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Miami, FL 33149 USA. EM serafy@noaa.gov RI Cooke, Steven/F-4193-2010 OI Cooke, Steven/0000-0002-5407-0659 FU National Oceanic and Atmospheric Administration's National Marine Fisheries Service (NMFS) offices of Protected Resources, Sustainable Fisheries, International Affairs, and Science and Technology; NMFS Southeast Fisheries Science Center; Guy Harvey Ocean Foundation and Guy Harvey Research Institute at Nova Southeastern University; International Seafood Sustainability Foundation; World Wildlife Fund; Fisheries Program; The Billfish Foundation; Ocean Smart; Florida Sea Grant; University of Miami's RJ Dunlap Marine Conservation Program and Rosenstiel School of Marine & Atmospheric Science; Tag-A-Giant FX We extend our deepest gratitude to the symposium's supporting sponsors whose contributions made every aspect of this symposium a reality. These included: National Oceanic and Atmospheric Administration's National Marine Fisheries Service (NMFS) offices of Protected Resources, Sustainable Fisheries, International Affairs, and Science and Technology; NMFS Southeast Fisheries Science Center; Guy Harvey Ocean Foundation and Guy Harvey Research Institute at Nova Southeastern University; International Seafood Sustainability Foundation; World Wildlife Fund, Fisheries Program; The Billfish Foundation; Ocean Smart; Florida Sea Grant; University of Miami's RJ Dunlap Marine Conservation Program and Rosenstiel School of Marine & Atmospheric Science; and Tag-A-Giant. A special thanks also to our international delegates B Chokesanguan, R Sagarminaga, and K Yokota, for helping to spread the word about our symposium to specialists in their regions. D DiCarlo superbly handled all logistics from the symposium's inception to its final execution. S Marks, D Die, I Holder, and I Diaz provided key support in symposium planning. We were assisted by numerous University of Miami graduate students and staff that helped make the event a success. Hook illustrations were produced by J Javech who worked from original diagrams kindly provided by G Sivertzen ("Dr. Hook"). Finally, we are grateful to all those who contributed papers, abstracts, and/or oral presentations their expertise, experience, and perspectives educated and inspired those who attended and will be invaluable as we face present and future challenges in fishery sustainability. NR 76 TC 26 Z9 29 U1 2 U2 22 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 2012 VL 88 IS 3 BP 371 EP 391 DI 10.5343/bms.2012.1038 PG 21 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 986DF UT WOS:000307320400001 ER PT J AU Epperly, SP Watson, JW Foster, DG Shah, AK AF Epperly, Sheryan P. Watson, John W. Foster, Daniel G. Shah, Arvind K. TI ANATOMICAL HOOKING LOCATION AND CONDITION OF ANIMALS CAPTURED WITH PELAGIC LONGLINES: THE GRAND BANKS EXPERIMENTS 2002-2003 SO BULLETIN OF MARINE SCIENCE LA English DT Article ID CIRCLE HOOKS; POSTRELEASE SURVIVAL; RECREATIONAL FISHERY; RELEASE FISHERIES; CATCH RATES; SEA-TURTLES; MORTALITY; MANAGEMENT; BYCATCH; TARGET AB Experiments were conducted on the Grand Banks of the North Atlantic Ocean during 2002-2003 to evaluate the effect of circle hooks and mackerel bait on pelagic longline catches and bycatch, and compare the treatments to the industry standards at the time. Circle hooks were 18/0, and both non-offset and 10 offset were used as separate treatments and compared to the 9/0 J-hook control hooks with 10 degrees-30 degrees offset. Bait treatment was mackerel (Scomber scombrus Linnaeus, 1758), which was compared to the squid control (Illex spp.). We analyzed the effects of hook (one J- and two circle hooks), bait (mackerel and squid), temperature, soak time, and animal length on anatomical hooking location for seven fish species and two sea turtle species. We also analyzed the effects of the same variables, inclusive and exclusive of hooking location, on the odds of boating a dead fish. We found that hook was one of the most important variables in predicting anatomical hooking location, and that soak time and hook and/or anatomical hooking location were important in predicting the odds of observing a dead animal boatside. The importance of the other variables differed by species, and for several species no models were significant for predicting hooking location or for predicting observed mortality. C1 [Epperly, Sheryan P.] NOAA, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Miami, FL 33149 USA. [Watson, John W.] NOAA, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA. [Shah, Arvind K.] Merck Res Labs, Rahway, NJ 07065 USA. RP Epperly, SP (reprint author), NOAA, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, 75 Virginia Beach Dr, Miami, FL 33149 USA. EM Sheryan.Epperly@noaa.gov NR 40 TC 16 Z9 17 U1 0 U2 10 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 2012 VL 88 IS 3 BP 513 EP 527 DI 10.5343/bms.2011.1083 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 986DF UT WOS:000307320400009 ER PT J AU Foster, DG Epperly, SP Shah, AK Watson, JW AF Foster, Daniel G. Epperly, Sheryan P. Shah, Arvind K. Watson, John W. TI EVALUATION OF HOOK AND BAIT TYPE ON THE CATCH RATES IN THE WESTERN NORTH ATLANTIC OCEAN PELAGIC LONGLINE FISHERY SO BULLETIN OF MARINE SCIENCE LA English DT Article ID CIRCLE HOOK; SEA-TURTLE; FISHING GEAR; BYCATCH; TARGET; TUNA; PERFORMANCE; MORTALITY AB Research was conducted in 2002 and 2003 by NOAA's National Marine Fisheries Service, Southeast Fisheries Science Center, to investigate changes in hook design and bait type to reduce the bycatch of sea turtles on pelagic longlines in the western North Atlantic Ocean. The effectiveness of 18/0-20/0 circle hooks and 10/0 Japanese tuna hooks with squid (Illex spp.) and mackerel bait (Scomber scombrus Linnaeus, 1758) was evaluated against the industry standard 9/0 J-hooks with squid bait with respect to reducing sea turtle and shark interactions while maintaining swordfish (Xiphias gladius Linnaeus, 1758) and tuna (Thunnus spp.) catch rates. In total, 973,734 hooks were deployed during the study. Individually, circle hooks and mackerel bait significantly reduced both loggerhead [Caretta caretta (Linnaeus, 1758)] and leatherback [Dermochelys coriacea (Vandelli, 1761)] sea turtle bycatch. The combination of 18/0 circle hooks with mackerel bait was even more effective for loggerhead sea turtles and had a significant increase in swordfish catch by weight. The combination 18/0 circle hooks with squid bait resulted in a significant decrease in the swordfish catch and a significant increase in the catch rate of blue shark [Prionace glauca (Linnaeus, 1758)], bluefin tuna [Thunnus thynnus (Linnaeus, 1758)1, and albacore tuna [Thunnus alalunga (Bonnaterre, 1788)]. With all hook types, mackerel bait resulted in a significant decrease in blue shark, bigeye tuna [Thunnus obesus (Lowe, 1839)], and albacore tuna, but significantly increased the catch of porbeagle [Lamna nasus (Bonnaterre, 1788)] and shortfin mako (Isurus oxyrinchus Rafinesque, 1810). C1 [Foster, Daniel G.; Watson, John W.] NOAA, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA. [Epperly, Sheryan P.] NOAA, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Miami, FL 33149 USA. [Shah, Arvind K.] Merck Res Labs, Rahway, NJ 07065 USA. RP Foster, DG (reprint author), NOAA, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, 3209 Frederic St, Pascagoula, MS 39567 USA. EM Daniel.G.Foster@noaa.gov NR 36 TC 17 Z9 17 U1 0 U2 27 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 2012 VL 88 IS 3 BP 529 EP 545 DI 10.5343/bms.2011.1081 PG 17 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 986DF UT WOS:000307320400010 ER PT J AU Richards, PM Epperly, SP Watson, JW Foster, DG Bergmann, CE Beideman, NR AF Richards, Paul M. Epperly, Sheryan P. Watson, John W. Foster, Daniel G. Bergmann, Charles E. Beideman, Nelson R. TI CAN CIRCLE HOOK OFFSET COMBINED WITH BAITING TECHNIQUE AFFECT CATCH AND BYCATCH IN PELAGIC LONGLINE FISHERIES? SO BULLETIN OF MARINE SCIENCE LA English DT Article ID WESTERN NORTH-ATLANTIC; WHITE MARLIN; SEA-TURTLES; POSTRELEASE SURVIVAL; FISHING GEAR; MORTALITY; RELEASE; RATES; PERFORMANCE; BEHAVIOR AB Circle hooks have become a standard requirement in many commercial longline fisheries in the United States, and are used increasingly worldwide. Circle hooks, when compared to J-hooks, are thought to reduce bycatch without significantly decreasing (and possibly increasing) catch of most target species. Circle hook offset and baiting technique are also thought to influence bycatch and mortality of species of concern, such as sea turtles and billfishes. We compared non-offset circle hooks to those with a 10 degrees offset and single or threaded baiting techniques in the United States Atlantic and Gulf of Mexico pelagic longline fishery. Offset and/or baiting techniques were compared within sets targeting one of three species independently: swordfish, Xiphias gladius Linnaeus, 1758, yellowfin tuna, Thunnus albacares (Bonnaterre, 1788), and bigeye tuna, Thunnus obesus (Lowe, 1839). Most comparisons of catch and bycatch did not differ between gears or techniques. In swordfish-directed sets, we found a 46% decline in catch of Atlantic sailfish when using 18/0 non-offset circle hooks single baited with mackerel compared to 18/0 10 offset circle hooks with threaded mackerel. In yellowfin tuna sets, single baiting significantly decreased target catch by 22% and escolar catch by 28%, compared to threaded baiting. We detected no significant effect of any of the offset or baiting treatments on the bycatch of sea turtles and most other species of concern due to the rarity of capture events. We conclude, in part, that bycatch mitigation research in other fisheries with larger detrimental population level impacts to species of concern may potentially yield greater conservation benefits. C1 [Richards, Paul M.; Epperly, Sheryan P.] Natl Ocean & Atmospher Assoc, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Miami, FL 33149 USA. [Watson, John W.; Foster, Daniel G.] Natl Ocean & Atmospher Assoc, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA. [Bergmann, Charles E.] Natl Ocean & Atmospher Assoc, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Pascagoula, MS 39568 USA. RP Richards, PM (reprint author), Natl Ocean & Atmospher Assoc, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, 75 Virginia Beach Dr, Miami, FL 33149 USA. EM paul.richards@noaa.gov FU National Marine Fisheries Service Cooperative Research Program [NA04NMF4540212] FX We thank the fishers, observers, and the Southeast Fisheries Science Center Pelagic Observer Program that made this research possible. Funding was provided by the National Marine Fisheries Service Cooperative Research Program, project NA04NMF4540212. We thank the organizers of the International Symposium on Circle Hooks, J Serafy and G Diaz; their encouragement and enthusiasm are infectious. NR 30 TC 3 Z9 3 U1 0 U2 25 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 2012 VL 88 IS 3 BP 589 EP 603 DI 10.5343/bms.2011.1085 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 986DF UT WOS:000307320400014 ER PT J AU Chan, KL Inan, OT Bhattacharya, S Marcu, O AF Chan, Kimberly L. Inan, Omer T. Bhattacharya, Sharmila Marcu, Oana TI Estimating the speed of Drosophila locomotion using an automated behavior detection and analysis system SO FLY LA English DT Article DE Drosophila; behavior; locomotor; speed; signal processing ID FLIGHT SPEED; MELANOGASTER; PERFORMANCE; FLIES; AGE AB A fundamental phenotypic trait in Drosophila melanogaster is the speed of movement. Its quantification in response to environmental and experimental factors is highly useful for behavioral and neurological studies. Quantifying this behavioral characteristic in freely moving flies is difficult, and many current systems are limited to evaluating the speed of movement of one fly at a time or rely on expensive, time-consuming methods. Here, we present a novel signal processing method of quantifying the speed of multiple flies using a system with automatic behavior detection and analysis that we previously developed to quantify general activity. By evaluating the shape of the signal wave from recordings of a live and simulated single fly, a metric for speed of movement was found. The feasibility of using this metric to estimate the speed of movement in a population of flies was then confirmed by evaluating recordings taken from populations of flies maintained at two different temperatures. The results were consistent with those reported in the literature. This method provides an automated way of measuring speed of locomotion in a fly population, which will further quantify fly behavioral responses to the environment. C1 [Inan, Omer T.] NASA, Ames Res Ctr, Ames Associates, Moffett Field, CA 94035 USA. [Chan, Kimberly L.] Univ Calif Berkeley, Dept Bioengn, Berkeley, CA 94720 USA. [Marcu, Oana] SETI Inst, Carl Sagan Ctr, Mountain View, CA USA. RP Inan, OT (reprint author), NASA, Ames Res Ctr, Ames Associates, Moffett Field, CA 94035 USA. EM oeinan@gmail.com; oana.marcu@nasa.gov RI Chan, Kimberly/M-8355-2013 OI Chan, Kimberly/0000-0002-3091-2073 FU Achieving Competence in Computing, Engineering, and Space Science Program; American Association for the Advancement of Science (AAAS); NASA Fundamental Space Biology [09-FSB09PROP-0022] FX K.L.C. was supported through the Achieving Competence in Computing, Engineering, and Space Science Program, funded by the American Association for the Advancement of Science (AAAS). The work was funded by a NASA Fundamental Space Biology grant 09-FSB09PROP-0022 to S.B. and O.M. NR 19 TC 1 Z9 1 U1 0 U2 11 PU LANDES BIOSCIENCE PI AUSTIN PA 1806 RIO GRANDE ST, AUSTIN, TX 78702 USA SN 1933-6934 J9 FLY JI Fly PD JUL-SEP PY 2012 VL 6 IS 3 BP 205 EP 210 DI 10.4161/fly.20987 PG 6 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 005HO UT WOS:000308741700011 PM 22878427 ER PT J AU Ciardo, G Segala, R AF Ciardo, Gianfranco Segala, Roberto TI Selected papers from QEST 2010 SO PERFORMANCE EVALUATION LA English DT Editorial Material C1 [Ciardo, Gianfranco] Univ Calif Riverside, Dept Comp Sci & Engn, Riverside, CA 92521 USA. [Ciardo, Gianfranco] Coll William & Mary, Williamsburg, VA USA. [Ciardo, Gianfranco] HP Labs, Palo Alto, CA USA. [Ciardo, Gianfranco] NASA, Langley Res Ctr, ICASE, Hampton, VA 23665 USA. [Ciardo, Gianfranco] Software Prod Consortium, Herndon, VA USA. [Ciardo, Gianfranco] Cselt SpA, Turin, Italy. [Segala, Roberto] Univ Verona, Dept Comp Sci, I-37100 Verona, Italy. [Segala, Roberto] Univ Bologna, I-40126 Bologna, Italy. RP Ciardo, G (reprint author), Univ Turin, I-10124 Turin, Italy. NR 0 TC 0 Z9 0 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5316 J9 PERFORM EVALUATION JI Perform. Eval. PD JUL-AUG PY 2012 VL 69 IS 7-8 SI SI BP 297 EP 298 DI 10.1016/j.peva.2012.06.002 PG 2 WC Computer Science, Hardware & Architecture; Computer Science, Theory & Methods SC Computer Science GA 996BM UT WOS:000308059000001 ER PT J AU Beauford, RE Arnold, SK Sears, D AF Beauford, R. E. Arnold, S. K. Sears, D. TI THE MACROSTRUCTURE OF THE SUTTER'S MILL METEORITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 75th Annual Meeting of the Meteoritical-Society CY AUG 12-17, 2012 CL Cairns, AUSTRALIA SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci C1 [Beauford, R. E.] Univ Arkansas, Fayetteville, AR 72701 USA. [Sears, D.] NASA, Ames Res Ctr, Washington, DC USA. EM rbeaufor@uark.edu; meteorhntr@aol.com; Derek.Sears@NASA.gov NR 2 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2012 VL 47 SU 1 SI SI BP A59 EP A59 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 987AV UT WOS:000307389700026 ER PT J AU Berger, EL Lauretta, DS Keller, LP AF Berger, E. L. Lauretta, D. S. Keller, L. P. TI THE THERMODYNAMIC PROPERTIES OF CUBANITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 75th Annual Meeting of the Meteoritical-Society CY AUG 12-17, 2012 CL Cairns, AUSTRALIA SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci ID CHONDRITES C1 [Lauretta, D. S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77573 USA. [Berger, E. L.; Keller, L. P.] Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM eve.l.berger@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 2 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 JUL PY 2012 VL 47 SU 1 SI SI BP A66 EP A66 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 987AV UT WOS:000307389700033 ER PT J AU Bussey, DBJ McGovern, JA Greenhagen, BT Paige, DA Cahill, JTS Siegler, M Spudis, PD AF Bussey, D. B. J. McGovern, J. A. Greenhagen, B. T. Paige, D. A. Cahill, J. T. S. Siegler, M. Spudis, P. D. TI GLOBAL CATALOGUE OF LUNAR PERMANENTLY SHADOWED REGIONS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 75th Annual Meeting of the Meteoritical-Society CY AUG 12-17, 2012 CL Cairns, AUSTRALIA SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci C1 [Bussey, D. B. J.; McGovern, J. A.; Cahill, J. T. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Greenhagen, B. T.; Siegler, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Paige, D. A.; Siegler, M.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Spudis, P. D.] Lunar & Planetary Inst, Houston, TX 77058 USA. RI Cahill, Joshua/I-3656-2012; Greenhagen, Benjamin/C-3760-2016 OI Cahill, Joshua/0000-0001-6874-5533; NR 4 TC 0 Z9 0 U1 0 U2 5 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 JUL PY 2012 VL 47 SU 1 SI SI BP A90 EP A90 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 987AV UT WOS:000307389700057 ER PT J AU Cartwright, JA Ott, U Mittlefehldt, DW Herrin, JS Mertzman, KR Mertzman, SA Peng, ZX Quinn, JE AF Cartwright, J. A. Ott, U. Mittlefehldt, D. W. Herrin, J. S. Mertzman, K. R. Mertzman, S. A. Peng, Z. X. Quinn, J. E. TI IN THE PURSUIT OF REGOLITHIC HOWARDITES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 75th Annual Meeting of the Meteoritical-Society CY AUG 12-17, 2012 CL Cairns, AUSTRALIA SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci C1 [Cartwright, J. A.; Ott, U.] MPIC, D-55128 Mainz, Germany. [Ott, U.] Univ Western Hungary, H-9700 Szombathely, Hungary. [Mittlefehldt, D. W.] NASA JSC, Houston, TX USA. [Herrin, J. S.; Peng, Z. X.; Quinn, J. E.] ESCG, Houston, TX USA. [Mertzman, K. R.; Mertzman, S. A.] Franklin & Marshall Coll, Lancaster, PA 17604 USA. EM julia.cartwright@mpic.de RI Cartwright, Julia/A-8470-2013 NR 7 TC 0 Z9 0 U1 0 U2 4 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 JUL PY 2012 VL