FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Lupu, RE
Scott, KS
Aguirre, JE
Aretxaga, I
Auld, R
Barton, E
Beelen, A
Bertoldi, F
Bock, JJ
Bonfield, D
Bradford, CM
Buttiglione, S
Cava, A
Clements, DL
Cooke, J
Cooray, A
Dannerbauer, H
Dariush, A
De Zotti, G
Dunne, L
Dye, S
Eales, S
Frayer, D
Fritz, J
Glenn, J
Hughes, DH
Ibar, E
Ivison, RJ
Jarvis, MJ
Kamenetzky, J
Kim, S
Lagache, G
Leeuw, L
Maddox, S
Maloney, PR
Matsuhara, H
Murphy, EJ
Naylor, BJ
Negrello, M
Nguyen, H
Omont, A
Pascale, E
Pohlen, M
Rigby, E
Rodighiero, G
Serjeant, S
Smith, D
Temi, P
Thompson, M
Valtchanov, I
Verma, A
Vieira, JD
Zmuidzinas, J
AF Lupu, R. E.
Scott, K. S.
Aguirre, J. E.
Aretxaga, I.
Auld, R.
Barton, E.
Beelen, A.
Bertoldi, F.
Bock, J. J.
Bonfield, D.
Bradford, C. M.
Buttiglione, S.
Cava, A.
Clements, D. L.
Cooke, J.
Cooray, A.
Dannerbauer, H.
Dariush, A.
De Zotti, G.
Dunne, L.
Dye, S.
Eales, S.
Frayer, D.
Fritz, J.
Glenn, J.
Hughes, D. H.
Ibar, E.
Ivison, R. J.
Jarvis, M. J.
Kamenetzky, J.
Kim, S.
Lagache, G.
Leeuw, L.
Maddox, S.
Maloney, P. R.
Matsuhara, H.
Murphy, E. J.
Naylor, B. J.
Negrello, M.
Nguyen, H.
Omont, A.
Pascale, E.
Pohlen, M.
Rigby, E.
Rodighiero, G.
Serjeant, S.
Smith, D.
Temi, P.
Thompson, M.
Valtchanov, I.
Verma, A.
Vieira, J. D.
Zmuidzinas, J.
TI MEASUREMENTS OF CO REDSHIFTS WITH Z-SPEC FOR LENSED SUBMILLIMETER
GALAXIES DISCOVERED IN THE H-ATLAS SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: distances and redshifts; galaxies: high-redshift; galaxies:
ISM-line: identification; submillimeter: galaxies
ID STAR-FORMING GALAXIES; GREEN-BANK-TELESCOPE; MOLECULAR
INTERSTELLAR-MEDIUM; SCIENCE DEMONSTRATION PHASE; DEGREE EXTRAGALACTIC
SURVEY; ORDER-STATISTICS; HERSCHEL-ATLAS; APM 08279+5255; WATER-VAPOR;
DUST TEMPERATURE
AB We present new observations from Z-Spec, a broadband 185-305 GHz spectrometer, of five submillimeter bright lensed sources selected from the Herschel-Astrophysical Terahertz Large Area Survey science demonstration phase catalog. We construct a redshift-finding algorithm using combinations of the signal to noise of all the lines falling in the Z-Spec bandpass to determine redshifts with high confidence, even in cases where the signal to noise in individual lines is low. We measure the dust continuum in all sources and secure CO redshifts for four out of five (z similar to 1.5-3). In one source, SDP. 17, we tentatively identify two independent redshifts and a water line, confirmed at z = 2.308. Our sources have properties characteristic of dusty starburst galaxies, with magnification-corrected star formation rates of 10(2-3) M-circle dot yr(-1). Lower limits for the dust masses (similar to a few 10(8) M-circle dot) and spatial extents (similar to 1 kpc equivalent radius) are derived from the continuum spectral energy distributions, corresponding to dust temperatures between 54 and 69 K. In the local thermodynamic equilibrium (LTE) approximation, we derive relatively low CO excitation temperatures (less than or similar to 100 K) and optical depths (tau less than or similar to 1). Performing a non-LTE excitation analysis using RADEX, we find that the CO lines measured by Z-Spec (from J = 4 -> 3 to 10 -> 9, depending on the galaxy) localize the best solutions to either a high-temperature/low-density region or a low/temperature/high-density region near the LTE solution, with the optical depth varying accordingly. Observations of additional CO lines, CO(1-0) in particular, are needed to constrain the non-LTE models.
C1 [Lupu, R. E.; Scott, K. S.; Aguirre, J. E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Aguirre, J. E.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico.
[Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Barton, E.; Cooke, J.; Cooray, A.; Kim, S.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Beelen, A.] Univ Paris 11, Inst Astrophys Spatiale Bat 121, F-91405 Orsay, France.
[Bertoldi, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Bock, J. J.; Bradford, C. M.; Naylor, B. J.; Nguyen, H.; Zmuidzinas, J.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J. J.; Bradford, C. M.; Vieira, J. D.; Zmuidzinas, J.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Bonfield, D.; Jarvis, M. J.; Thompson, M.] Univ Hertfordshire, Sci & Technol Res Ctr, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Buttiglione, S.; De Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Cava, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Cava, A.] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Tenerife, Spain.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Dept Phys, Astrophys Grp, London SW7 2AZ, England.
[Dannerbauer, H.] CEA DSM CNRS Univ Paris Diderot, Lab AIM, DAPNIA Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France.
[De Zotti, G.] Scuola Int Super Studi Avanzati, I-34136 Trieste, Italy.
[Maddox, S.; Rigby, E.; Smith, D.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Glenn, J.; Kamenetzky, J.; Maloney, P. R.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA.
[Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Lagache, G.] CNRS, F-91405 Orsay, France.
[Leeuw, L.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Leeuw, L.] SETI Inst, Mountain View, CA 94043 USA.
[Matsuhara, H.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan.
[Murphy, E. J.] Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Negrello, M.; Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Omont, A.] CNRS, F-75014 Paris, France.
[Omont, A.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
[Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[Valtchanov, I.] European Space Agcy, European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain.
[Verma, A.] Univ Oxford, Oxford OX1 3RH, England.
RP Lupu, RE (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
EM Roxana.E.Lupu@nasa.gov
RI Lupu, Roxana/P-9060-2014; Ivison, R./G-4450-2011; Cava,
Antonio/C-5274-2017;
OI Rodighiero, Giulia/0000-0002-9415-2296; Lupu,
Roxana/0000-0003-3444-5908; Ivison, R./0000-0001-5118-1313; Cava,
Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595;
Maddox, Stephen/0000-0001-5549-195X; Dye, Simon/0000-0002-1318-8343;
Smith, Daniel/0000-0001-9708-253X
FU NSF [AST-0807990, AST-0239270]; CSO NSF [AST-0838261]; NASA SARA
[NAGS-11911, NAGS-12788]; Research Corporation Award [RI0928]
FX We are indebted to the staff of the Caltech Submillimeter Observatory
for their unflagging support. This work was supported by NSF grant
AST-0807990 to J. Aguirre and by the CSO NSF Cooperative Agreement
AST-0838261. Support was provided to J. Kamenetzky by an NSF Graduate
Research Fellowship. Z-spec was constructed under NASA SARA grants
NAGS-11911 and NAGS-12788 and an NSF Career grant (AST-0239270) and a
Research Corporation Award (RI0928) to J. Glenn, in collaboration with
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration. We
acknowledge Peter Ade and his group for their filters and Lionel Duband
for the 3He/4He refrigerator in Z-Spec, and are grateful for their help
in the early integration of the instrument. R. L. thanks Tom Loredo for
useful discussions regarding the significance of the redshift
determination, and P. Papadopoulos for help improving the gas mass
discussion. R. L. also thanks the anonymous referee for the thorough
read and the helpful comments for improving the paper. We appreciate the
help of Robert Hanni and Jon Rodriguez with observing.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
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DI 10.1088/0004-637X/757/2/135
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500028
ER
PT J
AU Sazonov, S
Willner, SP
Goulding, AD
Hickox, RC
Gorjian, V
Werner, MW
Churazov, E
Krivonos, R
Revnivtsev, M
Sunyaev, R
Jones, C
Murray, SS
Vikhlinin, A
Fabian, AC
Forman, WR
AF Sazonov, S.
Willner, S. P.
Goulding, A. D.
Hickox, R. C.
Gorjian, V.
Werner, M. W.
Churazov, E.
Krivonos, R.
Revnivtsev, M.
Sunyaev, R.
Jones, C.
Murray, S. S.
Vikhlinin, A.
Fabian, A. C.
Forman, W. R.
TI CONTRIBUTION OF THE ACCRETION DISK, HOT CORONA, AND OBSCURING TORUS TO
THE LUMINOSITY OF SEYFERT GALAXIES: INTEGRAL AND SPITZER OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: active;
galaxies: Seyfert; infrared: galaxies; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE
BLACK-HOLES; X-RAY-EMISSION; ALL-SKY SURVEY; POLYCYCLIC
AROMATIC-HYDROCARBONS; SWIFT-BAT SURVEY; SIMILAR-TO 0.1;
SPACE-TELESCOPE; NEARBY GALAXIES
AB We estimate the relative contributions of the supermassive black hole (SMBH) accretion disk, corona, and obscuring torus to the bolometric luminosity of Seyfert galaxies, using Spitzer mid-infrared (MIR) observations of a complete sample of 68 nearby active galactic nuclei (AGNs) from the INTEGRAL all-sky hard X-ray (HX) survey. This is the first HX-selected (above 15 keV) sample of AGNs with complementary high angular resolution, high signal-to-noise, MIR data. Correcting for the host galaxy contribution, we find a correlation between HX and MIR luminosities: L-15 mu m alpha L-HX(0.74 +/- 0.06). Assuming that the observed MIR emission is radiation from an accretion disk reprocessed in a surrounding dusty torus that subtends a solid angle decreasing with increasing luminosity (as inferred from the declining fraction of obscured AGNs), the intrinsic disk luminosity, L-Disk, is approximately proportional to the luminosity of the corona in the 2-300 keV energy band, L-Corona, with the L-Disk/L-Corona ratio varying by a factor of 2.1 around a mean value of 1.6. This ratio is a factor of similar to 2 smaller than for typical quasars producing the cosmic X-ray background. Therefore, over three orders of magnitude in luminosity, HX radiation carries a large, and roughly comparable, fraction of the bolometric output of AGNs. We estimate the cumulative bolometric luminosity density of local AGNs at similar to(1-3) x 10(40) erg s(-1) Mpc(-3). Finally, the Compton temperature ranges between kT(c) approximate to 2 and approximate to 6 keV for nearby AGNs, compared to kT(c) approximate to 2 keV for typical quasars, confirming that radiative heating of interstellar gas can play an important role in regulating SMBH growth.
C1 [Sazonov, S.; Churazov, E.; Krivonos, R.; Revnivtsev, M.; Sunyaev, R.; Vikhlinin, A.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Sazonov, S.; Churazov, E.; Krivonos, R.; Sunyaev, R.; Forman, W. R.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Willner, S. P.; Goulding, A. D.; Jones, C.; Murray, S. S.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
[Gorjian, V.; Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Sazonov, S (reprint author), Russian Acad Sci, Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia.
RI Churazov, Eugene/A-7783-2013
FU Russian Academy of Sciences [P-21, OFN-16]; Scientific and educational
personnel of the innovative Russia [2012-1.2.2-12-000-1012-023]; Dynasty
Foundation; NASA; [RFBR 09-02-00867]; [RFBR 11-02-12271-ofi-m];
[NSh-5603.2012.2]
FX We thank the referee for helpful comments. This work is based on
observations made with the Spitzer Space Telescope, operated by the Jet
Propulsion Laboratory at Caltech under a contract with NASA, and with
INTEGRAL, an ESA project funded by ESA member states (especially the PI
countries: Denmark, France, Germany, Italy, Spain, and Switzerland),
Czech Republic and Poland, and with the participation of Russia and the
USA. The research made use of data obtained through the High Energy
Astrophysics Science Archive Research Center Online Service, provided by
the NASA/Goddard Space Flight Center. The research made use of grants
RFBR 09-02-00867, RFBR 11-02-12271-ofi-m, and NSh-5603.2012.2, programs
of the Russian Academy of Sciences P-21 and OFN-16, and the program
"Scientific and educational personnel of the innovative Russia
2009-2013" (2012-1.2.2-12-000-1012-023). S.S. acknowledges the support
of the Dynasty Foundation.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
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AR 181
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PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500074
ER
PT J
AU Sekanina, Z
Chodas, PW
AF Sekanina, Zdenek
Chodas, Paul W.
TI COMET C/2011 W3 (LOVEJOY): ORBIT DETERMINATION, OUTBURSTS,
DISINTEGRATION OF NUCLEUS, DUST-TAIL MORPHOLOGY, AND RELATIONSHIP TO NEW
CLUSTER OF BRIGHT SUNGRAZERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; comets: individual (comet of AD 467, X/1106 C1, comet
of 1314, X/1381 V1, C/1843 D1, C/1880 C1, C/1882 R1, C/1887 B1, C/1945
X1, C/1963 R1, C/1965 S1, C/1970 K1, D/1993 F2, C/2011 W3); methods:
data analysis
ID ELASTIC PROPERTIES; THERMAL-EXPANSION; DYNAMIC STRENGTH; WAVE
VELOCITIES; POROUS SILICON; TIDAL BREAKUP; KREUTZ SYSTEM; SOLAR;
FRAGMENTATION; DENSITY
AB We describe the physical and orbital properties of C/2011 W3. After surviving perihelion passage, the comet was observed to undergo major physical changes. The permanent loss of the nuclear condensation and the formation of a narrow spine tail were observed first at Malargue, Argentina, on December 20 and then systematically at Siding Spring, Australia. The process of disintegration culminated with a terminal fragmentation event on December 17.6 UT. The postperihelion dust tail, observed for similar to 3 months, was the product of activity over <2 days. The nucleus' breakup and crumbling were probably caused by thermal stress due to the penetration of the intense heat pulse deep into the nucleus' interior after perihelion. The same mechanism may be responsible for cascading fragmentation of sungrazers at large heliocentric distances. The delayed response to the hostile environment in the solar corona is at odds with the rubble-pile model, since the residual mass of the nucleus, estimated at similar to 10(12) g (equivalent to a sphere 150-200 m across) just before the terminal event, still possessed nontrivial cohesive strength. The high production rates of atomic oxygen, observed shortly after perihelion, are compatible with a subkilometer-sized nucleus. The spine tail-the product of the terminal fragmentation-was a synchronic feature, whose brightest part contained submillimeter-sized dust grains, released at velocities of up to 30 m s(-1). The loss of the nuclear condensation prevented an accurate orbital-period determination by traditional techniques. Since the missing nucleus must have been located on the synchrone, whose orientation and sunward tip have been measured, we compute the astrometric positions of this missing nucleus as the coordinates of the points of intersection of the spine tail's axis with the lines of forced orbital-period variation, derived from the orbital solutions based on high-quality preperihelion astrometry from the ground. The resulting orbit gives 698 +/- 2 yr for the osculating orbital period, showing that C/2011 W3 is the first member of the expected new, 21st-century cluster of bright Kreutz-system sungrazers, whose existence was predicted by these authors in 2007. From the spine tail's evolution, we determine that its measured tip, populated by dust particles 1-2 mm in diameter, receded antisunward from the computed position of the missing nucleus. The bizarre appearance of the comet's dust tail in images taken only hours after perihelion with the coronagraphs on board the SOHO and STEREO spacecraft is readily understood. The disconnection of the comet's head from the tail released before perihelion and an apparent activity attenuation near perihelion have a common cause-sublimation of all dust at heliocentric distances smaller than about 1.8 solar radii. The tail's brightness is strongly affected by forward scattering of sunlight by dust. From an initially broad range of particle sizes, the grains that were imaged the longest had a radiation-pressure parameter beta similar or equal to 0.6, diagnostic of submicron-sized silicate grains and consistent with the existence of the dust-free zone around the Sun. The role and place of C/2011 W3 in the hierarchy of the Kreutz system and its genealogy via a 14th-century parent suggest that it is indirectly related to the celebrated sungrazer X/1106 C1, which, just as the first-generation parent of C/2011 W3, split from a common predecessor during the previous return to perihelion.
C1 [Sekanina, Zdenek; Chodas, Paul W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sekanina, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Zdenek.Sekanina@jpl.nasa.gov; Paul.W.Chodas@jpl.nasa.gov
NR 95
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500020
ER
PT J
AU Shaposhnikov, N
Jahoda, K
Markwardt, C
Swank, J
Strohmayer, T
AF Shaposhnikov, Nikolai
Jahoda, Keith
Markwardt, Craig
Swank, Jean
Strohmayer, Tod
TI ADVANCES IN THE RXTE PROPORTIONAL COUNTER ARRAY CALIBRATION: NEARING THE
STATISTICAL LIMIT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: detectors; space vehicles: instruments
ID RAY-TIMING-EXPLORER
AB During its 16 years of service, the Rossi X-Ray Timing Explorer (RXTE) mission has provided an extensive archive of data, which will serve as a primary source of high cadence observations of variable X-ray sources for fast timing studies. It is, therefore, very important to have the most reliable calibration of RXTE instruments. The Proportional Counter Array (PCA) is the primary instrument on board RXTE which provides data in 3-50 keV energy range with submillisecond time resolution in up to 256 energy channels. In 2009, the RXTE team revised the response residual minimization method used to derive the parameters of the PCA physical model. The procedure is based on the residual minimization between the model spectrum for Crab Nebula emission and a calibration data set consisting of a number of spectra from the Crab and the on-board Am-241 calibration source, uniformly covering the whole RXTE mission operation period. The new method led to a much more effective model convergence and allowed for better understanding of the PCA energy-to-channel relationship. It greatly improved the response matrix performance. We describe the new version of the RXTE/PCA response generator PCARMF v11.7 (HEASOFT Release 6.7) along with the corresponding energy-to-channel conversion table (version e05v04) and their difference from the previous releases of PCA calibration. The new PCA response adequately represents the spectrum of the calibration sources and successfully predicts the energy of the narrow iron emission line in Cas-A throughout the RXTE mission.
C1 [Shaposhnikov, Nikolai] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Shaposhnikov, Nikolai] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Shaposhnikov, Nikolai; Jahoda, Keith; Markwardt, Craig; Swank, Jean; Strohmayer, Tod] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Shaposhnikov, N (reprint author), Univ Maryland, CRESST, College Pk, MD 20742 USA.
EM nikolai.v.shaposhnikov@nasa.gov
NR 8
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
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DI 10.1088/0004-637X/757/2/159
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500052
ER
PT J
AU Landis, GA
AF Landis, Geoffrey A.
TI Future Tense Fermi's Paradox and the End of the Universe
SO COMMUNICATIONS OF THE ACM
LA English
DT Editorial Material
C1 NASA, John Glenn Res Ctr, Cleveland, OH USA.
RP Landis, GA (reprint author), NASA, John Glenn Res Ctr, Cleveland, OH USA.
EM geoffrey.landis@nasa.gov
NR 0
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PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 0001-0782
J9 COMMUN ACM
JI Commun. ACM
PD OCT
PY 2012
VL 55
IS 10
BP 112
EP 112
DI 10.1145/2347736.2347760
PG 1
WC Computer Science, Hardware & Architecture; Computer Science, Software
Engineering; Computer Science, Theory & Methods
SC Computer Science
GA 012DN
UT WOS:000309215800029
ER
PT J
AU Kohlman, LW
Bail, JL
Roberts, GD
Salem, JA
Martin, RE
Binienda, WK
AF Kohlman, Lee W.
Bail, Justin L.
Roberts, Gary D.
Salem, Jonathan A.
Martin, Richard E.
Binienda, Wieslaw K.
TI A notched coupon approach for tensile testing of braided composites
SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING
LA English
DT Article
DE Fabrics/textiles; Polymer-matrix composites; Strength; Mechanical
testing
AB A notched coupon geometry was evaluated as a method for tensile testing of 2D triaxial braid composites. Edge initiated shear failure has been observed in transverse tension tests using straight-sided coupons based on ASTM D3039. The notched coupon was designed to reduce the effects of edge initiated failure and produce the desired tensile failure. A limited set of tests were performed with partial pressurization of tubes to determine the transverse tensile strength in the absence of edge initiated failure. The transverse strength measured with the notched coupons was considerably higher than the straight-sided coupons, comparable to the tube results, and closer to the maximum possible strength based on maximum fiber strain. Further investigations of the effects of the observed biaxial stress state and stress concentrations in the notched geometry are needed. Published by Elsevier Ltd.
C1 [Kohlman, Lee W.; Roberts, Gary D.; Salem, Jonathan A.] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Kohlman, Lee W.; Binienda, Wieslaw K.] Univ Akron, Akron, OH 44325 USA.
[Bail, Justin L.] Ohio Aerosp Inst, Cleveland, OH USA.
[Martin, Richard E.] Cleveland State Univ, Cleveland, OH 44115 USA.
RP Kohlman, LW (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
EM lee.w.kohlman@nasa.gov
FU NASA GSRP [NNX09AK92H]
FX Partial funding for this work was provided through a NASA GSRP Grant
#NNX09AK92H.
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1359-835X
J9 COMPOS PART A-APPL S
JI Compos. Pt. A-Appl. Sci. Manuf.
PD OCT
PY 2012
VL 43
IS 10
SI SI
BP 1680
EP 1688
DI 10.1016/j.compositesa.2011.12.013
PG 9
WC Engineering, Manufacturing; Materials Science, Composites
SC Engineering; Materials Science
GA 011GJ
UT WOS:000309152700006
ER
PT J
AU Xia, ZH
Sujidkul, T
Niu, JB
Smith, CE
Morscher, GN
AF Xia, Zhenhai
Sujidkul, Thanyawalai
Niu, Jianbing
Smith, Craig E.
Morscher, Gregory N.
TI Modeling of electromechanical behavior of woven SiC/SiC composites
SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING
LA English
DT Article
DE Ceramic-matrix composites (CMCs); Electrical properties; Mechanical
properties; Computational modeling
ID CERAMIC-MATRIX COMPOSITES; FIBER-REINFORCED COMPOSITES;
ELECTRICAL-RESISTANCE; DAMAGE DETECTION; CFRP COMPOSITES; IN-SITU;
CRACKING; FRACTURE; MECHANICS; STRENGTH
AB A coupled electro-mechanical model was developed to predict the mechanical behavior of woven SiC/SiC ceramic matrix composites and electrical resistance response to mechanical damages in the composites. The matrix is explicitly included in the model such that the matrix cracking and fiber break can be linked to the electrical resistance change during loading. The results show that the electrical resistance increases linearly with an increase of matrix crack density and the number of fiber breaks. The predictions are compared to the experimental results on 2D woven SiC/SiC ceramic composites. With proper materials parameters input, the models can accurately predict the stress-strain curve and electrical resistance change during the loading. The model is further compared to an analytical solution of electromechanical coupling to get an insight into the electrical-mechanical interaction mechanisms in the composites. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Xia, Zhenhai; Niu, Jianbing] Univ N Texas, Dept Mat Sci & Engn, Denton, TX 76203 USA.
[Xia, Zhenhai; Niu, Jianbing] Univ N Texas, Dept Chem, Denton, TX 76203 USA.
[Sujidkul, Thanyawalai; Morscher, Gregory N.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
[Smith, Craig E.] NASA, Glenn Res Ctr, Ceram Branch, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
RP Xia, ZH (reprint author), Univ N Texas, Dept Mat Sci & Engn, Denton, TX 76203 USA.
EM Zhenhai.Xia@unt.edu
FU NASA Glenn Research Center ARMD Hypersonics program [NNX07AN56H]; Navy
SBIR; NSF [CMMI-0825990]
FX We would like to thank the NASA Glenn Research Center ARMD Hypersonics
program for the support of the graduate student research program under
contract NNX07AN56H and the Glenn Research Center Ceramics branch for
use of their research facilities. The project is also supported
partially by Navy SBIR and NSF (CMMI-0825990).
NR 30
TC 3
Z9 3
U1 1
U2 11
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1359-835X
J9 COMPOS PART A-APPL S
JI Compos. Pt. A-Appl. Sci. Manuf.
PD OCT
PY 2012
VL 43
IS 10
SI SI
BP 1730
EP 1737
DI 10.1016/j.compositesa.2012.03.020
PG 8
WC Engineering, Manufacturing; Materials Science, Composites
SC Engineering; Materials Science
GA 011GJ
UT WOS:000309152700011
ER
PT J
AU Christophe, B
Spilker, LJ
Anderson, JD
Andre, N
Asmar, SW
Aurnou, J
Banfield, D
Barucci, A
Bertolami, O
Bingham, R
Brown, P
Cecconi, B
Courty, JM
Dittus, H
Fletcher, LN
Foulon, B
Francisco, F
Gil, PJS
Glassmeier, KH
Grundy, W
Hansen, C
Helbert, J
Helled, R
Hussmann, H
Lamine, B
Lammerzahl, C
Lamy, L
Lehoucq, R
Lenoir, B
Levy, A
Orton, G
Paramos, J
Poncy, J
Postberg, F
Progrebenko, SV
Reh, KR
Reynaud, S
Robert, C
Samain, E
Saur, J
Sayanagi, KM
Schmitz, N
Selig, H
Sohl, F
Spilker, TR
Srama, R
Stephan, K
Touboul, P
Wolf, P
AF Christophe, B.
Spilker, L. J.
Anderson, J. D.
Andre, N.
Asmar, S. W.
Aurnou, J.
Banfield, D.
Barucci, A.
Bertolami, O.
Bingham, R.
Brown, P.
Cecconi, B.
Courty, J. -M.
Dittus, H.
Fletcher, L. N.
Foulon, B.
Francisco, F.
Gil, P. J. S.
Glassmeier, K. H.
Grundy, W.
Hansen, C.
Helbert, J.
Helled, R.
Hussmann, H.
Lamine, B.
Laemmerzahl, C.
Lamy, L.
Lehoucq, R.
Lenoir, B.
Levy, A.
Orton, G.
Paramos, J.
Poncy, J.
Postberg, F.
Progrebenko, S. V.
Reh, K. R.
Reynaud, S.
Robert, C.
Samain, E.
Saur, J.
Sayanagi, K. M.
Schmitz, N.
Selig, H.
Sohl, F.
Spilker, T. R.
Srama, R.
Stephan, K.
Touboul, P.
Wolf, P.
TI OSS (Outer Solar System): a fundamental and planetary physics mission to
Neptune, Triton and the Kuiper Belt
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Fundamental physics; Deep space gravity; Neptune; Triton; Kuiper Belt
object
ID MAGNETIC-FIELD MEASUREMENTS; RADIO SCIENCE OBSERVATIONS;
POST-EINSTEINIAN TESTS; FLUXGATE MAGNETOMETER; DARK ENERGY;
ELECTROSTATIC ACCELEROMETER; INTERIOR STRUCTURE; SUBSURFACE OCEANS;
DOPPLER TRACKING; CASSINI RADIO
AB The present OSS (Outer Solar System) mission continues a long and bright tradition by associating the communities of fundamental physics and planetary sciences in a single mission with ambitious goals in both domains. OSS is an M-class mission to explore the Neptune system almost half a century after the flyby of the Voyager 2 spacecraft. Several discoveries were made by Voyager 2, including the Great Dark Spot (which has now disappeared) and Triton's geysers. Voyager 2 revealed the dynamics of Neptune's atmosphere and found four rings and evidence of ring arcs above Neptune. Benefiting from a greatly improved instrumentation, a mission as OSS would result in a striking advance in the study of the farthest planet of the solar system. Furthermore, OSS would provide a unique opportunity to visit a selected Kuiper Belt object subsequent to the passage of the Neptunian system. OSS would help consolidate the hypothesis of the origin of Triton as a Kuiper Belt object captured by Neptune, and to improve our knowledge on the formation of the solar system. The OSS probe would carry instruments allowing precise tracking of the spacecraft during the cruise. It would facilitate the best possible tests of the laws of gravity in deep space. These objectives are important for fundamental physics, as they test General Relativity, our current theoretical description of gravitation, but also for cosmology, astrophysics and planetary science, as General Relativity is used as a tool in all these domains. In particular, the models of solar system formation uses General Relativity to describe the crucial role of gravity. OSS is proposed as an international cooperation between ESA and NASA, giving the capability for ESA to launch an M-class mission towards the farthest planet of the solar system, and to a Kuiper Belt object. The proposed mission profile would allow to deliver a 500 kg class spacecraft. The design of the probe is mainly constrained by the deep space gravity test in order to minimize the perturbation of the accelerometer measurement.
C1 [Christophe, B.; Foulon, B.; Lenoir, B.; Levy, A.; Robert, C.; Touboul, P.] ONERA French Aerosp Lab, F-92322 Chatillon, France.
[Spilker, L. J.; Anderson, J. D.; Asmar, S. W.; Orton, G.; Reh, K. R.; Spilker, T. R.] NASA, JPL, Pasadena, CA USA.
[Andre, N.] Univ Toulouse 3, CNRS, IRAP, F-31062 Toulouse, France.
[Aurnou, J.; Helled, R.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Banfield, D.] Cornell Univ, Ithaca, NY USA.
[Barucci, A.; Cecconi, B.; Lamy, L.] Univ Paris Diderot, Univ Paris 06, CNRS,Lab Etud Spatiales & Instrumentat Astrophys, Observ Paris, F-92195 Meudon, France.
[Bertolami, O.] Univ Porto, P-4100 Oporto, Portugal.
[Bingham, R.] RAL, Chilton, Oxon, England.
[Brown, P.] Univ London Imperial Coll Sci Technol & Med, London, England.
[Courty, J. -M.; Lamine, B.; Reynaud, S.] CNRS, LKB, Paris, France.
[Dittus, H.] DLR Inst Space Syst, Bremen, Germany.
[Fletcher, L. N.] Univ Oxford, Oxford, England.
[Francisco, F.; Gil, P. J. S.; Paramos, J.] Univ Tecn Lisboa, Inst Super Tecn, P-1096 Lisbon, Portugal.
[Glassmeier, K. H.] Tech Univ Carolo Wilhelmina Braunschweig, D-38106 Braunschweig, Germany.
[Grundy, W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Hansen, C.] PSI, Tucson, AZ USA.
[Helbert, J.; Hussmann, H.; Schmitz, N.; Sohl, F.; Stephan, K.] DLR Inst Planetary Res, Berlin, Germany.
[Laemmerzahl, C.; Selig, H.] Univ Bremen, ZARM, D-28359 Bremen, Germany.
[Lehoucq, R.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Poncy, J.] Thales Alenia Space, Cannes, France.
[Postberg, F.] Heidelberg Univ, Heidelberg, Germany.
[Progrebenko, S. V.] Joint Inst VLBI Europe, Dwingeloo, Netherlands.
[Samain, E.] GeoAzur, Observ Cote Azur, Nice, France.
[Saur, J.] Univ Cologne, D-50931 Cologne, Germany.
[Sayanagi, K. M.] Hampton Univ Virginia, Hampton, VA USA.
[Srama, R.] Univ Stuttgart, IRS, Stuttgart, Germany.
[Srama, R.] MPIK, Heidelberg, Germany.
[Wolf, P.] UPMC, CNRS, Observ Paris, LNE SYRTE, Paris, France.
RP Christophe, B (reprint author), ONERA French Aerosp Lab, F-92322 Chatillon, France.
EM bruno.christophe@onera.fr
RI Francisco, Frederico/J-1718-2012; Lamine, Brahim/J-8907-2012; Gil,
Paulo/B-7272-2012; Paramos, Jorge/J-3440-2013; Fletcher,
Leigh/D-6093-2011; Reynaud, Serge/J-8061-2014; Laemmerzahl,
Claus/P-3552-2016;
OI Francisco, Frederico/0000-0003-3014-0963; Lamine,
Brahim/0000-0002-9416-2320; Gil, Paulo/0000-0003-2183-6221; Paramos,
Jorge/0000-0001-9853-9431; Fletcher, Leigh/0000-0001-5834-9588; Reynaud,
Serge/0000-0002-1494-696X; Laemmerzahl, Claus/0000-0002-8276-5415;
Bertolami, Orfeu/0000-0002-7672-0560; Banfield, Don/0000-0003-2664-0164;
Helbert, Jorn/0000-0001-5346-9505
FU CNES (France)
FX This proposal was supported by CNES (France) through a phase 0 study
managed by E. Hinglais.
NR 145
TC 25
Z9 25
U1 1
U2 30
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 203
EP 242
DI 10.1007/s10686-012-9309-y
PG 40
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600004
ER
PT J
AU Oberst, J
Lainey, V
Le Poncin-Lafitte, C
Dehant, V
Rosenblatt, P
Ulamec, S
Biele, J
Spurmann, J
Kahle, R
Klein, V
Schreiber, U
Schlicht, A
Rambaux, N
Laurent, P
Noyelles, B
Foulon, B
Zakharov, A
Gurvits, L
Uchaev, D
Murchie, S
Reed, C
Turyshev, SG
Gil, J
Graziano, M
Willner, K
Wickhusen, K
Pasewaldt, A
Wahlisch, M
Hoffmann, H
AF Oberst, Juergen
Lainey, Valery
Le Poncin-Lafitte, Christophe
Dehant, Veronique
Rosenblatt, Pascal
Ulamec, Stephan
Biele, Jens
Spurmann, Joern
Kahle, Ralph
Klein, Volker
Schreiber, Ulrich
Schlicht, Anja
Rambaux, Nicolas
Laurent, Philippe
Noyelles, Benoit
Foulon, Bernard
Zakharov, Alexander
Gurvits, Leonid
Uchaev, Denis
Murchie, Scott
Reed, Cheryl
Turyshev, Slava G.
Gil, Jesus
Graziano, Mariella
Willner, Konrad
Wickhusen, Kai
Pasewaldt, Andreas
Waehlisch, Marita
Hoffmann, Harald
TI GETEMME-a mission to explore the Martian satellites and the fundamentals
of solar system physics
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Cosmic Vision; Mars; Phobos; Deimos; Laser Ranging; Fundamental physics;
Lander; Electric propulsion
ID DOPPLER TRACKING; PHOBOS; DEIMOS; MARS; SURFACE; BALLOONS; PHILAE;
BODIES; MOONS; BODY
AB GETEMME (Gravity, Einstein's Theory, and Exploration of the Martian Moons' Environment), a mission which is being proposed in ESA's Cosmic Vision program, shall be launched for Mars on a Soyuz Fregat in 2020. The spacecraft will initially rendezvous with Phobos and Deimos in order to carry out a comprehensive mapping and characterization of the two satellites and to deploy passive Laser retro-reflectors on their surfaces. In the second stage of the mission, the spacecraft will be transferred into a lower 1500-km Mars orbit, to carry out routine Laser range measurements to the reflectors on Phobos and Deimos. Also, asynchronous two-way Laser ranging measurements between the spacecraft and stations of the ILRS (International Laser Ranging Service) on Earth are foreseen. An onboard accelerometer will ensure a high accuracy for the spacecraft orbit determination. The inversion of all range and accelerometer data will allow us to determine or improve dramatically on a host of dynamic parameters of the Martian satellite system. From the complex motion and rotation of Phobos and Deimos we will obtain clues on internal structures and the origins of the satellites. Also, crucial data on the time-varying gravity field of Mars related to climate variation and internal structure will be obtained. Ranging measurements will also be essential to improve on several parameters in fundamental physics, such as the Post-Newtonian parameter beta as well as time-rate changes of the gravitational constant and the Lense-Thirring effect. Measurements by GETEMME will firmly embed Mars and its satellites into the Solar System reference frame.
C1 [Oberst, Juergen; Wickhusen, Kai; Pasewaldt, Andreas; Waehlisch, Marita; Hoffmann, Harald] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Willner, Konrad] Tech Univ Berlin, Berlin, Germany.
[Lainey, Valery; Rambaux, Nicolas; Noyelles, Benoit] Observ Paris, IMCCE, F-75014 Paris, France.
[Dehant, Veronique; Rosenblatt, Pascal] Royal Observ Belgium, Brussels, Belgium.
[Ulamec, Stephan; Biele, Jens] German Aerosp Ctr DLR, Cologne, Germany.
[Spurmann, Joern; Kahle, Ralph] German Aerosp Ctr DLR, Oberpfaffenhofen, Germany.
[Klein, Volker] Kayser Threde GmbH, Munich, Germany.
[Schreiber, Ulrich; Schlicht, Anja] Wettzell Observ, Wettzell, Germany.
[Foulon, Bernard] French Natl Aerosp Res Ctr, Chatillon, France.
[Zakharov, Alexander] Russian Acad Sci IKI, Space Res Inst, Moscow, Russia.
[Gurvits, Leonid] Joint Inst VLBI Europe JIVE, Dwingeloo, Netherlands.
[Gurvits, Leonid] Delft Univ Technol, Dept Astrodynam & Space Missions, Delft, Netherlands.
[Uchaev, Denis] Moscow State Univ Geodesy & Cartog MIIGAiK, Moscow, Russia.
[Murchie, Scott; Reed, Cheryl] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Turyshev, Slava G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Gil, Jesus; Graziano, Mariella] Innovating Solut, Gmv Madrid, Spain.
RP Oberst, J (reprint author), German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM juergen.oberst@dlr.de
RI Uchaev, Denis/A-8207-2014; Murchie, Scott/E-8030-2015; Noyelles,
Benoit/Q-1767-2015; Schreiber, Karl/H-5378-2011
OI Uchaev, Denis/0000-0002-8324-8305; Murchie, Scott/0000-0002-1616-8751;
Noyelles, Benoit/0000-0003-4106-8741; Schreiber,
Karl/0000-0002-3775-5058
NR 61
TC 10
Z9 10
U1 0
U2 10
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 243
EP 271
DI 10.1007/s10686-012-9307-0
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600005
ER
PT J
AU Teriaca, L
Andretta, V
Auchere, F
Brown, CM
Buchlin, E
Cauzzi, G
Culhane, JL
Curdt, W
Davila, JM
Del Zanna, G
Doschek, GA
Fineschi, S
Fludra, A
Gallagher, PT
Green, L
Harra, LK
Imada, S
Innes, D
Kliem, B
Korendyke, C
Mariska, JT
Martinez-Pillet, V
Parenti, S
Patsourakos, S
Peter, H
Poletto, L
Rutten, RJ
Schuhle, U
Siemer, M
Shimizu, T
Socas-Navarro, H
Solanki, SK
Spadaro, D
Trujillo-Bueno, J
Tsuneta, S
Dominguez, SV
Vial, JC
Walsh, R
Warren, HP
Wiegelmann, T
Winter, B
Young, P
AF Teriaca, Luca
Andretta, Vincenzo
Auchere, Frederic
Brown, Charles M.
Buchlin, Eric
Cauzzi, Gianna
Culhane, J. Len
Curdt, Werner
Davila, Joseph M.
Del Zanna, Giulio
Doschek, George A.
Fineschi, Silvano
Fludra, Andrzej
Gallagher, Peter T.
Green, Lucie
Harra, Louise K.
Imada, Shinsuke
Innes, Davina
Kliem, Bernhard
Korendyke, Clarence
Mariska, John T.
Martinez-Pillet, Valentin
Parenti, Susanna
Patsourakos, Spiros
Peter, Hardi
Poletto, Luca
Rutten, Robert J.
Schuehle, Udo
Siemer, Martin
Shimizu, Toshifumi
Socas-Navarro, Hector
Solanki, Sami K.
Spadaro, Daniele
Trujillo-Bueno, Javier
Tsuneta, Saku
Dominguez, Santiago Vargas
Vial, Jean-Claude
Walsh, Robert
Warren, Harry P.
Wiegelmann, Thomas
Winter, Berend
Young, Peter
TI LEMUR: Large European module for solar Ultraviolet Research
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Sun: atmosphere; Space vehicles: instruments; Techniques: spectroscopy;
ESA cosmic vision
ID HELIOSPHERIC MAGNETIC-FIELDS; EUV IMAGING SPECTROMETER; ACTIVE REGIONS;
DOPPLER-SHIFT; LOOP OSCILLATIONS; CORONAL LOOPS; POLAR PLUMES; WIND;
HINODE; OUTFLOWS
AB The solar outer atmosphere is an extremely dynamic environment characterized by the continuous interplay between the plasma and the magnetic field that generates and permeates it. Such interactions play a fundamental role in hugely diverse astrophysical systems, but occur at scales that cannot be studied outside the solar system. Understanding this complex system requires concerted, simultaneous solar observations from the visible to the vacuum ultraviolet (VUV) and soft X-rays, at high spatial resolution (between 0.1'' and 0.3''), at high temporal resolution (on the order of 10 s, i.e., the time scale of chromospheric dynamics), with a wide temperature coverage (0.01 MK to 20 MK, from the chromosphere to the flaring corona), and the capability of measuring magnetic fields through spectropolarimetry at visible and near-infrared wavelengths. Simultaneous spectroscopic measurements sampling the entire temperature range are particularly important. These requirements are fulfilled by the Japanese Solar-C mission (Plan B), composed of a spacecraft in a geosynchronous orbit with a payload providing a significant improvement of imaging and spectropolarimetric capabilities in the UV, visible, and near-infrared with respect to what is available today and foreseen in the near future. The Large European Module for solar Ultraviolet Research (LEMUR), described in this paper, is a large VUV telescope feeding a scientific payload of high-resolution imaging spectrographs and cameras. LEMUR consists of two major components: a VUV solar telescope with a 30 cm diameter mirror and a focal length of 3.6 m, and a focal-plane package composed of VUV spectrometers covering six carefully chosen wavelength ranges between 170 and 1270 . The LEMUR slit covers 280'' on the Sun with 0.14'' per pixel sampling. In addition, LEMUR is capable of measuring mass flows velocities (line shifts) down to 2 km s (-aEuro parts per thousand 1) or better. LEMUR has been proposed to ESA as the European contribution to the Solar C mission.
C1 [Teriaca, Luca; Curdt, Werner; Innes, Davina; Peter, Hardi; Schuehle, Udo; Solanki, Sami K.; Wiegelmann, Thomas] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Andretta, Vincenzo] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Auchere, Frederic; Buchlin, Eric; Vial, Jean-Claude] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Brown, Charles M.; Doschek, George A.; Korendyke, Clarence; Mariska, John T.; Warren, Harry P.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Cauzzi, Gianna] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Culhane, J. Len; Green, Lucie; Harra, Louise K.; Dominguez, Santiago Vargas; Winter, Berend] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Del Zanna, Giulio] Univ Cambridge, Cambridge CB3 0WA, England.
[Fineschi, Silvano] INAF Osservatorio Astron Torino, Pino Torinese, Italy.
[Fludra, Andrzej] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Gallagher, Peter T.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland.
[Imada, Shinsuke; Shimizu, Toshifumi] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Kliem, Bernhard] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Martinez-Pillet, Valentin; Socas-Navarro, Hector; Trujillo-Bueno, Javier] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Parenti, Susanna] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Patsourakos, Spiros] Univ Ioannina, Dept Phys, Astrogeophys Sect, GR-45110 Ioannina, Greece.
[Poletto, Luca] CNR Inst Photon & Nanotechnol, Padua, Italy.
[Rutten, Robert J.] Sterrekundig Inst, NL-3508 TA Utrecht, Netherlands.
[Siemer, Martin] DLR Inst Space Syst, Bremen, Germany.
[Spadaro, Daniele] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Tsuneta, Saku] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Walsh, Robert] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England.
[Young, Peter] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
RP Teriaca, L (reprint author), Max Planck Inst Sonnensyst Forsch, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM teriaca@mps.mpg.de
RI Solanki, Sami/E-2487-2013; Gallagher, Peter/C-7717-2011
OI Solanki, Sami/0000-0002-3418-8449; Gallagher, Peter/0000-0001-9745-0400
NR 34
TC 10
Z9 10
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 273
EP 309
DI 10.1007/s10686-011-9274-x
PG 37
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600006
ER
PT J
AU Tinetti, G
Beaulieu, JP
Henning, T
Meyer, M
Micela, G
Ribas, I
Stam, D
Swain, M
Krause, O
Ollivier, M
Pace, E
Swinyard, B
Aylward, A
van Boekel, R
Coradini, A
Encrenaz, T
Snellen, I
Zapatero-Osorio, MR
Bouwman, J
Cho, JYK
du Foresto, VC
Guillot, T
Lopez-Morales, M
Mueller-Wodarg, I
Palle, E
Selsis, F
Sozzetti, A
Ade, PAR
Achilleos, N
Adriani, A
Agnor, CB
Afonso, C
Prieto, CA
Bakos, G
Barber, RJ
Barlow, M
Batista, V
Bernath, P
Bezard, B
Borde, P
Brown, LR
Cassan, A
Cavarroc, C
Ciaravella, A
Cockell, C
Coustenis, A
Danielski, C
Decin, L
De Kok, R
Demangeon, O
Deroo, P
Doel, P
Drossart, P
Fletcher, LN
Focardi, M
Forget, F
Fossey, S
Fouque, P
Frith, J
Galand, M
Gaulme, P
Hernandez, JIG
Grasset, O
Grassi, D
Grenfell, JL
Griffin, MJ
Griffith, CA
Grozinger, U
Guedel, M
Guio, P
Hainaut, O
Hargreaves, R
Hauschildt, PH
Heng, K
Heyrovsky, D
Hueso, R
Irwin, P
Kaltenegger, L
Kervella, P
Kipping, D
Koskinen, TT
Kovacs, G
La Barbera, A
Lammer, H
Lellouch, E
Leto, G
Valverde, MAL
Lopez-Puertas, M
Lovis, C
Maggio, A
Maillard, JP
Prado, JM
Marquette, JB
Martin-Torres, FJ
Maxted, P
Miller, S
Molinari, S
Montes, D
Moro-Martin, A
Moses, JI
Mousis, O
Tuong, NN
Nelson, R
Orton, GS
Pantin, E
Pascale, E
Pezzuto, S
Pinfield, D
Poretti, E
Prinja, R
Prisinzano, L
Rees, JM
Reiners, A
Samuel, B
Sanchez-Lavega, A
Forcada, JS
Sasselov, D
Savini, G
Sicardy, B
Smith, A
Stixrude, L
Strazzulla, G
Tennyson, J
Tessenyi, M
Vasisht, G
Vinatier, S
Viti, S
Waldmann, I
White, GJ
Widemann, T
Wordsworth, R
Yelle, R
Yung, Y
Yurchenko, SN
AF Tinetti, G.
Beaulieu, J. P.
Henning, T.
Meyer, M.
Micela, G.
Ribas, I.
Stam, D.
Swain, M.
Krause, O.
Ollivier, M.
Pace, E.
Swinyard, B.
Aylward, A.
van Boekel, R.
Coradini, A.
Encrenaz, T.
Snellen, I.
Zapatero-Osorio, M. R.
Bouwman, J.
Cho, J. Y-K.
du Foresto, V. Coude
Guillot, T.
Lopez-Morales, M.
Mueller-Wodarg, I.
Palle, E.
Selsis, F.
Sozzetti, A.
Ade, P. A. R.
Achilleos, N.
Adriani, A.
Agnor, C. B.
Afonso, C.
Allende Prieto, C.
Bakos, G.
Barber, R. J.
Barlow, M.
Batista, V.
Bernath, P.
Bezard, B.
Borde, P.
Brown, L. R.
Cassan, A.
Cavarroc, C.
Ciaravella, A.
Cockell, C.
Coustenis, A.
Danielski, C.
Decin, L.
De Kok, R.
Demangeon, O.
Deroo, P.
Doel, P.
Drossart, P.
Fletcher, L. N.
Focardi, M.
Forget, F.
Fossey, S.
Fouque, P.
Frith, J.
Galand, M.
Gaulme, P.
Gonzalez Hernandez, J. I.
Grasset, O.
Grassi, D.
Grenfell, J. L.
Griffin, M. J.
Griffith, C. A.
Groezinger, U.
Guedel, M.
Guio, P.
Hainaut, O.
Hargreaves, R.
Hauschildt, P. H.
Heng, K.
Heyrovsky, D.
Hueso, R.
Irwin, P.
Kaltenegger, L.
Kervella, P.
Kipping, D.
Koskinen, T. T.
Kovacs, G.
La Barbera, A.
Lammer, H.
Lellouch, E.
Leto, G.
Lopez Valverde, M. A.
Lopez-Puertas, M.
Lovis, C.
Maggio, A.
Maillard, J. P.
Maldonado Prado, J.
Marquette, J. B.
Martin-Torres, F. J.
Maxted, P.
Miller, S.
Molinari, S.
Montes, D.
Moro-Martin, A.
Moses, J. I.
Mousis, O.
Nguyen Tuong, N.
Nelson, R.
Orton, G. S.
Pantin, E.
Pascale, E.
Pezzuto, S.
Pinfield, D.
Poretti, E.
Prinja, R.
Prisinzano, L.
Rees, J. M.
Reiners, A.
Samuel, B.
Sanchez-Lavega, A.
Sanz Forcada, J.
Sasselov, D.
Savini, G.
Sicardy, B.
Smith, A.
Stixrude, L.
Strazzulla, G.
Tennyson, J.
Tessenyi, M.
Vasisht, G.
Vinatier, S.
Viti, S.
Waldmann, I.
White, G. J.
Widemann, T.
Wordsworth, R.
Yelle, R.
Yung, Y.
Yurchenko, S. N.
TI EChO
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Exoplanets; Planetary atmospheres; Space mission
ID TRANSITING EXTRASOLAR PLANET; EXOPLANET HD 209458B; UPSILON ANDROMEDAE
B; EARTH-LIKE PLANETS; MU-M; TRANSMISSION SPECTRUM; M-DWARFS; PHASE
CURVE; ATMOSPHERE; 189733B
AB A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO-the Exoplanet Characterisation Observatory-is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. The use of passive cooling, few moving parts and well established technology gives a low-risk and potentially long-lived mission. EChO will build on observations by Hubble, Spitzer and ground-based telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. However, EChO's configuration and specifications are designed to study a number of systems in a consistent manner that will eliminate the ambiguities affecting prior observations. EChO will simultaneously observe a broad enough spectral region-from the visible to the mid-infrared-to constrain from one single spectrum the temperature structure of the atmosphere, the abundances of the major carbon and oxygen bearing species, the expected photochemically-produced species and magnetospheric signatures. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules and retrieve the composition and temperature structure of planetary atmospheres. The target list for EChO includes planets ranging from Jupiter-sized with equilibrium temperatures T (eq) up to 2,000 K, to those of a few Earth masses, with T (eq) \u223c 300 K. The list will include planets with no Solar System analog, such as the recently discovered planets GJ1214b, whose density lies between that of terrestrial and gaseous planets, or the rocky-iron planet 55 Cnc e, with day-side temperature close to 3,000 K. As the number of detected exoplanets is growing rapidly each year, and the mass and radius of those detected steadily decreases, the target list will be constantly adjusted to include the most interesting systems. We have baselined a dispersive spectrograph design covering continuously the 0.4-16 mu m spectral range in 6 channels (1 in the visible, 5 in the InfraRed), which allows the spectral resolution to be adapted from several tens to several hundreds, depending on the target brightness. The instrument will be mounted behind a 1.5 m class telescope, passively cooled to 50 K, with the instrument structure and optics passively cooled to \u223c45 K. EChO will be placed in a grand halo orbit around L2. This orbit, in combination with an optimised thermal shield design, provides a highly stable thermal environment and a high degree of visibility of the sky to observe repeatedly several tens of targets over the year. Both the baseline and alternative designs have been evaluated and no critical items with Technology Readiness Level (TRL) less than 4-5 have been identified. We have also undertaken a first-order cost and development plan analysis and find that EChO is easily compatible with the ESA M-class mission framework.
C1 [Tinetti, G.; Aylward, A.; Achilleos, N.; Barber, R. J.; Barlow, M.; Danielski, C.; Doel, P.; Fossey, S.; Guio, P.; Miller, S.; Prinja, R.; Savini, G.; Stixrude, L.; Tennyson, J.; Tessenyi, M.; Viti, S.; Waldmann, I.; Yurchenko, S. N.] UCL, London, England.
[Beaulieu, J. P.; Batista, V.; Cassan, A.; Maillard, J. P.; Marquette, J. B.] Inst Astrophys Paris, Paris, France.
[Henning, T.; Krause, O.; van Boekel, R.; Bouwman, J.; Afonso, C.; Groezinger, U.; Kaltenegger, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Meyer, M.; Heng, K.] ETH, Zurich, Switzerland.
[Micela, G.; Coradini, A.; Sozzetti, A.; Adriani, A.; Ciaravella, A.; Grassi, D.; La Barbera, A.] INAF, Turin, Italy.
[Ribas, I.] IEEC CSIC, Inst Ciencies Espai, Barcelona, Spain.
[Stam, D.; De Kok, R.] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Swain, M.; Brown, L. R.; Deroo, P.; Orton, G. S.; Vasisht, G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Ollivier, M.; Borde, P.; Cavarroc, C.; Demangeon, O.; Gaulme, P.; Samuel, B.] Inst Astrophys Spatiale, Orsay, France.
[Pace, E.; Focardi, M.; Molinari, S.] Un Firenze, Florence, Italy.
[Swinyard, B.] UCL RAL, Didcot, Oxon, England.
[Encrenaz, T.; du Foresto, V. Coude; Bezard, B.; Coustenis, A.; Drossart, P.; Kervella, P.; Lellouch, E.; Nguyen Tuong, N.; Rees, J. M.; Sicardy, B.; Vinatier, S.; Widemann, T.] Observ Paris, LESIA, Meudon, France.
[Snellen, I.] Leiden Univ, Leiden, Netherlands.
[Zapatero-Osorio, M. R.; Martin-Torres, F. J.; Moro-Martin, A.; Sanz Forcada, J.] CAB, Madrid, Spain.
[Cho, J. Y-K.; Agnor, C. B.; Nelson, R.] QMUL, London, England.
[Guillot, T.] Observ Nice, Nice, France.
[Lopez-Morales, M.] IEEC, Bellaterra, Spain.
[Mueller-Wodarg, I.; Galand, M.] Univ London Imperial Coll Sci Technol & Med, London, England.
[Palle, E.; Allende Prieto, C.; Gonzalez Hernandez, J. I.] IAC, Tenerife, Spain.
[Selsis, F.] Un Bordeaux, Bordeaux, France.
[Ade, P. A. R.; Griffin, M. J.; Pascale, E.] Cardiff Univ, Cardiff, S Glam, Wales.
[Bernath, P.; Hargreaves, R.] Univ York, York YO10 5DD, N Yorkshire, England.
[Cockell, C.] ROE, Edinburgh, Midlothian, Scotland.
[Decin, L.] IvS, Louvain, Belgium.
[Focardi, M.; Irwin, P.] Univ Oxford, Oxford, England.
[Forget, F.; Wordsworth, R.] LMD, Paris, France.
[Fouque, P.] Obs MIP, Toulouse, France.
[Frith, J.; Pinfield, D.] UH, Hatfield, Herts, England.
[Grasset, O.] Un Nantes, Nantes, France.
[Grenfell, J. L.] TUB, Berlin, Germany.
[Griffith, C. A.; Koskinen, T. T.; Yelle, R.] UoA, Tucson, AZ USA.
[Guedel, M.] Un Vienna, Vienna, Austria.
[Hainaut, O.] ESO, La Silla, Chile.
[Hauschildt, P. H.] HS, Hamburg, Germany.
[Heyrovsky, D.] CU Prague, Prague, Czech Republic.
[Hueso, R.; Sanchez-Lavega, A.] EHU Bilbao, Bilbao, Spain.
[Kipping, D.; Sasselov, D.] CfA UCL, CfA, Cambridge, MA USA.
[Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary.
[Lammer, H.] Un Graz, Graz, Austria.
[Leto, G.; Strazzulla, G.] INAF OACt, Catania, Italy.
[Lopez Valverde, M. A.; Lopez-Puertas, M.] IAA CSIC, Granada, Spain.
[Lovis, C.] Observ Geneva, Geneva, Switzerland.
[Maggio, A.] INAF OAPa, Palermo, Italy.
[Maldonado Prado, J.] UAM, Madrid, Spain.
[Maxted, P.] Un Keele, Keele, Staffs, England.
[Montes, D.] UCM, Madrid, Spain.
[Moses, J. I.] SSI, Seabrook, TX USA.
[Mousis, O.] Obs Besancon, Besancon, France.
[Pantin, E.] CEA, Saclay, France.
[Pezzuto, S.] IFSI INAF, Florence, Italy.
[Poretti, E.] INAF OAMi, Milan, Italy.
[Prisinzano, L.] INAF OAPa, Palermo, Italy.
[Reiners, A.] IAG, Gottinghen, Germany.
[Smith, A.] MSSL, London, England.
[White, G. J.] OU RAL, Didcot, Oxon, England.
RP Tinetti, G (reprint author), UCL, London, England.
EM g.tinetti@ucl.ac.uk; beaulieu@iap.fr; henning@mpia.de;
mmeyer@phys.ethz.ch; giusi@astropa.inaf.it; iribas@ieec.uab.es;
d.m.stam@sron.nl; swain@s383.jpl.nasa.gov
RI Guedel, Manuel/C-8486-2015; Martin-Torres, Francisco Javier/G-6329-2015;
Leto, Giuseppe/N-3355-2015; Maggio, Antonio/P-5700-2015; Yurchenko,
Sergey/G-9929-2012; Stixrude, Lars/C-5625-2012; Molinari,
Sergio/O-4095-2016; Zapatero Osorio, Maria Rosa/C-2744-2017;
Sanz-Forcada, Jorge/C-3176-2017; Ribas, Ignasi/M-2134-2014; Gonzalez
Hernandez, Jonay I./L-3556-2014; Mueller-Wodarg, Ingo/M-9945-2014;
Heyrovsky, David/A-2031-2015; Guio, Patrick/A-6271-2008; Bernath,
Peter/B-6567-2012; Barlow, Michael/A-5638-2009; Focardi,
Mauro/B-7880-2013; Moses, Julianne/I-2151-2013; Tennyson,
Jonathan/I-2222-2012; Lopez Puertas, Manuel/M-8219-2013; Montes,
David/B-9329-2014; Fletcher, Leigh/D-6093-2011;
OI Poretti, Ennio/0000-0003-1200-0473; Irwin, Patrick/0000-0002-6772-384X;
Lopez-Valverde, M. A./0000-0002-7989-4267; Grassi,
Davide/0000-0003-1653-3066; Hueso, Ricardo/0000-0003-0169-123X; Tinetti,
Giovanna/0000-0001-6058-6654; Pezzuto, Stefano/0000-0001-7852-1971;
Achilleos, Nicholas/0000-0002-5886-3509; LA BARBERA,
ANTONINO/0000-0002-5880-8913; Sozzetti, Alessandro/0000-0002-7504-365X;
Adriani, Alberto/0000-0003-4998-8008; Sanchez-Lavega,
Agustin/0000-0001-7355-1522; Guedel, Manuel/0000-0001-9818-0588;
Martin-Torres, Francisco Javier/0000-0001-6479-2236; Leto,
Giuseppe/0000-0002-0040-5011; Maggio, Antonio/0000-0001-5154-6108;
Yurchenko, Sergey/0000-0001-9286-9501; Stixrude,
Lars/0000-0003-3778-2432; Molinari, Sergio/0000-0002-9826-7525; Zapatero
Osorio, Maria Rosa/0000-0001-5664-2852; Sanz-Forcada,
Jorge/0000-0002-1600-7835; Ribas, Ignasi/0000-0002-6689-0312; Gonzalez
Hernandez, Jonay I./0000-0002-0264-7356; Mueller-Wodarg,
Ingo/0000-0001-6308-7826; Heyrovsky, David/0000-0002-5198-5343; Guio,
Patrick/0000-0002-1607-5862; Bernath, Peter/0000-0002-1255-396X; Barlow,
Michael/0000-0002-3875-1171; Focardi, Mauro/0000-0002-3806-4283; Moses,
Julianne/0000-0002-8837-0035; Tennyson, Jonathan/0000-0002-4994-5238;
Lopez Puertas, Manuel/0000-0003-2941-7734; Montes,
David/0000-0002-7779-238X; Fletcher, Leigh/0000-0001-5834-9588; Savini,
Giorgio/0000-0003-4449-9416
NR 83
TC 90
Z9 91
U1 0
U2 49
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 311
EP 353
DI 10.1007/s10686-012-9303-4
PG 43
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600007
ER
PT J
AU Boccaletti, A
Schneider, J
Traub, W
Lagage, PO
Stam, D
Gratton, R
Trauger, J
Cahoy, K
Snik, F
Baudoz, P
Galicher, R
Reess, JM
Mawet, D
Augereau, JC
Patience, J
Kuchner, M
Wyatt, M
Pantin, E
Maire, AL
Verinaud, C
Ronayette, S
Dubreuil, D
Min, M
Rodenhuis, M
Mesa, D
Belikov, R
Guyon, O
Tamura, M
Murakami, N
Beerer, IM
AF Boccaletti, Anthony
Schneider, Jean
Traub, Wes
Lagage, Pierre-Olivier
Stam, Daphne
Gratton, Raffaele
Trauger, John
Cahoy, Kerri
Snik, Frans
Baudoz, Pierre
Galicher, Raphael
Reess, Jean-Michel
Mawet, Dimitri
Augereau, Jean-Charles
Patience, Jenny
Kuchner, Marc
Wyatt, Mark
Pantin, Eric
Maire, Anne-Lise
Verinaud, Christophe
Ronayette, Samuel
Dubreuil, Didier
Min, Michiel
Rodenhuis, Michiel
Mesa, Dino
Belikov, Russ
Guyon, Olivier
Tamura, Motohide
Murakami, Naoshi
Beerer, Ingrid Mary
CA SPICES Team
TI SPICES: spectro-polarimetric imaging and characterization of
exoplanetary systems
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Exoplanets; High contrast imaging
ID PHASE-MASK CORONAGRAPH; EXTRASOLAR PLANET; DAYSIDE SPECTRUM; HR 8799;
LIGHT; EARTH; DISK; SIGNATURES; METHANE
AB SPICES (Spectro-Polarimetric Imaging and Characterization of Exoplanetary Systems) is a five-year M-class mission proposed to ESA Cosmic Vision. Its purpose is to image and characterize long-period extrasolar planets and circumstellar disks in the visible (450-900 nm) at a spectral resolution of about 40 using both spectroscopy and polarimetry. By 2020/2022, present and near-term instruments will have found several tens of planets that SPICES will be able to observe and study in detail. Equipped with a 1.5 m telescope, SPICES can preferentially access exoplanets located at several AUs (0.5-10 AU) from nearby stars (< 25 pc) with masses ranging from a few Jupiter masses to Super Earths (similar to 2 Earth radii, similar to 10 M-aS center dot) as well as circumstellar disks as faint as a few times the zodiacal light in the Solar System.
C1 [Boccaletti, Anthony; Baudoz, Pierre; Galicher, Raphael; Reess, Jean-Michel; Maire, Anne-Lise] Observ Paris, LESIA, Meudon, France.
[Schneider, Jean] Observ Paris, LUTH, Meudon, France.
[Traub, Wes; Trauger, John; Mawet, Dimitri] NASA, JPL, Pasadena, CA USA.
[Lagage, Pierre-Olivier; Pantin, Eric; Ronayette, Samuel; Dubreuil, Didier] SAp CEA, Saclay, France.
[Stam, Daphne] SRON, Utrecht, Netherlands.
[Gratton, Raffaele] Astron Observ Padova, INAF, I-35122 Padua, Italy.
[Cahoy, Kerri; Belikov, Russ] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Snik, Frans] Sterrekundig Inst, NL-3508 TA Utrecht, Netherlands.
[Augereau, Jean-Charles; Verinaud, Christophe] IPAG, Grenoble, France.
[Patience, Jenny] Univ Exeter, Exeter, Devon, England.
[Kuchner, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wyatt, Mark] Univ Cambridge, Cambridge, England.
[Min, Michiel; Rodenhuis, Michiel] Univ Utrecht, Utrecht, Netherlands.
[Guyon, Olivier] Univ Arizona, Tucson, AZ USA.
[Guyon, Olivier] Subaru Telescope NAOJ, Hilo, HI USA.
[Tamura, Motohide] NAOJ, Tokyo, Japan.
[Murakami, Naoshi] Hokkaido Univ, Sapporo, Hokkaido 060, Japan.
[Beerer, Ingrid Mary] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA.
RP Boccaletti, A (reprint author), Observ Paris, LESIA, Meudon, France.
EM anthony.boccaletti@obspm.fr
FU CNES
FX We would like to thanks H. Boithias, E. Sein at ASTRIUM France for their
technical support and A. Laurens, O. Lamarle at CNES for both financial
and technical support during this ESA Cosmic Vision proposal study. We
are also grateful to the referee for relevant comments which helped to
improve this paper.
NR 46
TC 16
Z9 16
U1 1
U2 15
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 355
EP 384
DI 10.1007/s10686-012-9290-5
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600008
ER
PT J
AU Malbet, F
Leger, A
Shao, M
Goullioud, R
Lagage, PO
Brown, AGA
Cara, C
Durand, G
Eiroa, C
Feautrier, P
Jakobsson, B
Hinglais, E
Kaltenegger, L
Labadie, L
Lagrange, AM
Laskar, J
Liseau, R
Lunine, J
Maldonado, J
Mercier, M
Mordasini, C
Queloz, D
Quirrenbach, A
Sozzetti, A
Traub, W
Absil, O
Alibert, Y
Andrei, AH
Arenou, F
Beichman, C
Chelli, A
Cockell, CS
Duvert, G
Forveille, T
Garcia, PJV
Hobbs, D
Krone-Martins, A
Lammer, H
Meunier, N
Minardi, S
de Almeida, AM
Rambaux, N
Raymond, S
Rottgering, HJA
Sahlmann, J
Schuller, PA
Segransan, D
Selsis, F
Surdej, J
Villaver, E
White, GJ
Zinnecker, H
AF Malbet, Fabien
Leger, Alain
Shao, Michael
Goullioud, Renaud
Lagage, Pierre-Olivier
Brown, Anthony G. A.
Cara, Christophe
Durand, Gilles
Eiroa, Carlos
Feautrier, Philippe
Jakobsson, Bjoern
Hinglais, Emmanuel
Kaltenegger, Lisa
Labadie, Lucas
Lagrange, Anne-Marie
Laskar, Jacques
Liseau, Rene
Lunine, Jonathan
Maldonado, Jesus
Mercier, Manuel
Mordasini, Christoph
Queloz, Didier
Quirrenbach, Andreas
Sozzetti, Alessandro
Traub, Wesley
Absil, Olivier
Alibert, Yann
Andrei, Alexandre Humberto
Arenou, Frederic
Beichman, Charles
Chelli, Alain
Cockell, Charles S.
Duvert, Gilles
Forveille, Thierry
Garcia, Paulo J. V.
Hobbs, David
Krone-Martins, Alberto
Lammer, Helmut
Meunier, Nadege
Minardi, Stefano
de Almeida, Andre Moitinho
Rambaux, Nicolas
Raymond, Sean
Roettgering, Huub J. A.
Sahlmann, Johannes
Schuller, Peter A.
Segransan, Damien
Selsis, Franck
Surdej, Jean
Villaver, Eva
White, Glenn J.
Zinnecker, Hans
TI High precision astrometry mission for the detection and characterization
of nearby habitable planetary systems with the Nearby Earth Astrometric
Telescope (NEAT)
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Exoplanets; Planetary systems; Planetary formation; Astrometry; Space
Mission
ID JITTER
AB A complete census of planetary systems around a volume-limited sample of solar-type stars (FGK dwarfs) in the Solar neighborhood (d a parts per thousand currency signaEuro parts per thousand 15 pc) with uniform sensitivity down to Earth-mass planets within their Habitable Zones out to several AUs would be a major milestone in extrasolar planets astrophysics. This fundamental goal can be achieved with a mission concept such as NEAT-the Nearby Earth Astrometric Telescope. NEAT is designed to carry out space-borne extremely-high-precision astrometric measurements at the 0.05 mu as (1 sigma) accuracy level, sufficient to detect dynamical effects due to orbiting planets of mass even lower than Earth's around the nearest stars. Such a survey mission would provide the actual planetary masses and the full orbital geometry for all the components of the detected planetary systems down to the Earth-mass limit. The NEAT performance limits can be achieved by carrying out differential astrometry between the targets and a set of suitable reference stars in the field. The NEAT instrument design consists of an off-axis parabola single-mirror telescope (D = 1 m), a detector with a large field of view located 40 m away from the telescope and made of 8 small movable CCDs located around a fixed central CCD, and an interferometric calibration system monitoring dynamical Young's fringes originating from metrology fibers located at the primary mirror. The mission profile is driven by the fact that the two main modules of the payload, the telescope and the focal plane, must be located 40 m away leading to the choice of a formation flying option as the reference mission, and of a deployable boom option as an alternative choice. The proposed mission architecture relies on the use of two satellites, of about 700 kg each, operating at L2 for 5 years, flying in formation and offering a capability of more than 20,000 reconfigurations. The two satellites will be launched in a stacked configuration using a Soyuz ST launch vehicle. The NEAT primary science program will encompass an astrometric survey of our 200 closest F-, G- and K-type stellar neighbors, with an average of 50 visits each distributed over the nominal mission duration. The main survey operation will use approximately 70% of the mission lifetime. The remaining 30% of NEAT observing time might be allocated, for example, to improve the characterization of the architecture of selected planetary systems around nearby targets of specific interest (low-mass stars, young stars, etc.) discovered by Gaia, ground-based high-precision radial-velocity surveys, and other programs. With its exquisite, surgical astrometric precision, NEAT holds the promise to provide the first thorough census for Earth-mass planets around stars in the immediate vicinity of our Sun.
C1 [Malbet, Fabien; Feautrier, Philippe; Lagrange, Anne-Marie; Chelli, Alain; Duvert, Gilles; Forveille, Thierry; Meunier, Nadege] UJF Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble 9, France.
[Leger, Alain] Univ Paris 11, CNRS INSU, IAS, UMR 8617, F-91405 Orsay, France.
[Shao, Michael; Goullioud, Renaud; Traub, Wesley] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lagage, Pierre-Olivier; Cara, Christophe; Durand, Gilles] Univ Paris Diderot, Lab AIM, CEA IRFU CNRS INSU, CEA Saclay,UMR 7158, F-91191 Gif Sur Yvette, France.
[Brown, Anthony G. A.; Roettgering, Huub J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Eiroa, Carlos; Maldonado, Jesus; Villaver, Eva] Univ Autonoma Madrid, Fac Ciencias, Dpto Fis Teor, E-28049 Madrid, Spain.
[Jakobsson, Bjoern] Swedish Space Corp, S-17104 Solna, Sweden.
[Hinglais, Emmanuel] CNES, Ctr Spatial Toulouse, F-31401 Toulouse 9, France.
[Kaltenegger, Lisa; Mordasini, Christoph] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Labadie, Lucas] Univ Cologne, I Phys Inst, D-50937 Cologne, Germany.
[Laskar, Jacques; Rambaux, Nicolas] UPMC Paris 6, Observ Paris, IMCCE, CNRS INSU,UMR 8028, F-75014 Paris, France.
[Liseau, Rene] Chalmers, S-41296 Gothenburg, Sweden.
[Lunine, Jonathan] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Mercier, Manuel] Thales Alenia Space, F-06150 Cannes, France.
[Queloz, Didier; Sahlmann, Johannes; Segransan, Damien] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Quirrenbach, Andreas] Univ Heidelberg, Landessternwarte, D-69117 Heidelberg, Germany.
[Sozzetti, Alessandro; Andrei, Alexandre Humberto] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy.
[Absil, Olivier; Surdej, Jean] Univ Liege, Dept Astrophys Geophys & Oceanographie, B-4000 Sart Tilman Par Liege, Belgium.
[Alibert, Yann] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Alibert, Yann] Univ Besancon, Inst UTINAM, Observ Besancon, CNRS INSU,UMR 6213, F-25010 Besancon, France.
[Andrei, Alexandre Humberto] Minist Ciencia & Tecnol, Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[Arenou, Frederic] Univ Paris 07, GEPI, Observ Paris, CNRS INSU,UMR 8111, F-92190 Meudon, France.
[Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, IPAC, Pasadena, CA 91125 USA.
[Cockell, Charles S.] Open Univ, Dept Phys & Astron, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
[Garcia, Paulo J. V.] Univ Porto, Fac Engn, Dept Engn Fsica, Lab SIM, P-4200465 Oporto, Portugal.
[Hobbs, David] Lund Univ, Lund Observ, S-22100 Lund, Sweden.
[Krone-Martins, Alberto] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil.
[Krone-Martins, Alberto; Raymond, Sean; Selsis, Franck] Univ Bordeaux, Lab Astrophys Bordeaux, Observ Aquitain Sci Univers, CNRS INSU,UMR 5804, F-33271 Floirac, France.
[Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Minardi, Stefano] Univ Jena, Inst Appl Phys, D-07743 Jena, Germany.
[Krone-Martins, Alberto; de Almeida, Andre Moitinho] Univ Lisbon, Fac Ciencias, SIM, P-1749016 Lisbon, Portugal.
[Schuller, Peter A.] Univ Paris 07, Observ Paris, CNRS INSU, LESIA,UMR 8109, F-92190 Meudon, France.
[White, Glenn J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[White, Glenn J.] CCLRC Rutherford Appleton Lab, Rutherford Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
[Zinnecker, Hans] Univ Stuttgart, Inst Raumfahrtsyst, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Zinnecker, Hans] NASA Ames, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
RP Malbet, F (reprint author), UJF Grenoble 1, IPAG, CNRS INSU, UMR 5274, BP 53, F-38041 Grenoble 9, France.
EM Fabien.Malbet@obs.ujf-grenoble.fr
RI Laskar, Jacques/E-1098-2011; Arenou, Frederic/B-1846-2014; Moitinho de
Almeida, Andre/L-1624-2015; Valente Garcia, Paulo Jorge/B-8933-2009;
Krone-Martins, Alberto/B-8635-2014;
OI Laskar, Jacques/0000-0003-2634-789X; Arenou,
Frederic/0000-0003-2837-3899; Moitinho de Almeida,
Andre/0000-0003-0822-5995; Valente Garcia, Paulo
Jorge/0000-0002-1678-3535; Sozzetti, Alessandro/0000-0002-7504-365X;
Krone-Martins, Alberto/0000-0002-2308-6623; Minardi,
Stefano/0000-0002-7563-103X; Sahlmann, Johannes/0000-0001-9525-3673;
Villaver, Eva/0000-0003-4936-9418; Absil, Olivier/0000-0002-4006-6237
FU Centre National des Etudes Spatiales (CNES); Jet Propulsion Laboratory
(JPL); Thales Alenia Space (TAS); Swedish Space Corporation (SSC)
FX This work has benefited support from the Centre National des Etudes
Spatiales (CNES), the Jet Propulsion Laboratory (JPL), Thales Alenia
Space (TAS) and Swedish Space Corporation (SSC).
NR 15
TC 19
Z9 20
U1 0
U2 21
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 385
EP 413
DI 10.1007/s10686-011-9246-1
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600009
ER
PT J
AU Feroci, M
Stella, L
van der Klis, M
Courvoisier, TJL
Hernanz, M
Hudec, R
Santangelo, A
Walton, D
Zdziarski, A
Barret, D
Belloni, T
Braga, J
Brandt, S
Budtz-Jorgensen, C
Campana, S
den Herder, JW
Huovelin, J
Israel, GL
Pohl, M
Ray, P
Vacchi, A
Zane, S
Argan, A
Attina, P
Bertuccio, G
Bozzo, E
Campana, R
Chakrabarty, D
Costa, E
De Rosa, A
Del Monte, E
Di Cosimo, S
Donnarumma, I
Evangelista, Y
Haas, D
Jonker, P
Korpela, S
Labanti, C
Malcovati, P
Mignani, R
Muleri, F
Rapisarda, M
Rashevsky, A
Rea, N
Rubini, A
Tenzer, C
Wilson-Hodge, C
Winter, B
Wood, K
Zampa, G
Zampa, N
Abramowicz, MA
Alpar, MA
Altamirano, D
Alvarez, JM
Amati, L
Amoros, C
Antonelli, LA
Artigue, R
Azzarello, P
Bachetti, M
Baldazzi, G
Barbera, M
Barbieri, C
Basa, S
Baykal, A
Belmont, R
Boirin, L
Bonvicini, V
Burderi, L
Bursa, M
Cabanac, C
Cackett, E
Caliandro, GA
Casella, P
Chaty, S
Chenevez, J
Coe, MJ
Collura, A
Corongiu, A
Covino, S
Cusumano, G
D'Amico, F
Dall'Osso, S
De Martino, D
De Paris, G
Di Persio, G
Di Salvo, T
Done, C
Dovciak, M
Drago, A
Ertan, U
Fabiani, S
Falanga, M
Fender, R
Ferrando, P
Ferreira, DD
Fraser, G
Frontera, F
Fuschino, F
Galvez, JL
Gandhi, P
Giommi, P
Godet, O
Gogus, E
Goldwurm, A
Gotz, D
Grassi, M
Guttridge, P
Hakala, P
Henri, G
Hermsen, W
Horak, J
Hornstrup, A
in't Zand, JJM
Isern, J
Kalemci, E
Kanbach, G
Karas, V
Kataria, D
Kennedy, T
Klochkov, D
Kluzniak, W
Kokkotas, K
Kreykenbohm, I
Krolik, J
Kuiper, L
Kuvvetli, I
Kylafis, N
Lattimer, JM
Lazzarotto, F
Leahy, D
Lebrun, F
Lin, D
Lund, N
Maccarone, T
Malzac, J
Marisaldi, M
Martindale, A
Mastropietro, M
McClintock, J
McHardy, I
Mendez, M
Mereghetti, S
Miller, MC
Mineo, T
Morelli, E
Morsink, S
Motch, C
Motta, S
Munoz-Darias, T
Naletto, G
Neustroev, V
Nevalainen, J
Olive, JF
Orio, M
Orlandini, M
Orleanski, P
Ozel, F
Pacciani, L
Paltani, S
Papadakis, I
Papitto, A
Patruno, A
Pellizzoni, A
Petracek, V
Petri, J
Petrucci, PO
Phlips, B
Picolli, L
Possenti, A
Psaltis, D
Rambaud, D
Reig, P
Remillard, R
Rodriguez, J
Romano, P
Romanova, M
Schanz, T
Schmid, C
Segreto, A
Shearer, A
Smith, A
Smith, PJ
Soffitta, P
Stergioulas, N
Stolarski, M
Stuchlik, Z
Tiengo, A
Torres, D
Torok, G
Turolla, R
Uttley, P
Vaughan, S
Vercellone, S
Waters, R
Watts, A
Wawrzaszek, R
Webb, N
Wilms, J
Zampieri, L
Zezas, A
Ziolkowski, J
AF Feroci, M.
Stella, L.
van der Klis, M.
Courvoisier, T. J. -L.
Hernanz, M.
Hudec, R.
Santangelo, A.
Walton, D.
Zdziarski, A.
Barret, D.
Belloni, T.
Braga, J.
Brandt, S.
Budtz-Jorgensen, C.
Campana, S.
den Herder, J. -W.
Huovelin, J.
Israel, G. L.
Pohl, M.
Ray, P.
Vacchi, A.
Zane, S.
Argan, A.
Attina, P.
Bertuccio, G.
Bozzo, E.
Campana, R.
Chakrabarty, D.
Costa, E.
De Rosa, A.
Del Monte, E.
Di Cosimo, S.
Donnarumma, I.
Evangelista, Y.
Haas, D.
Jonker, P.
Korpela, S.
Labanti, C.
Malcovati, P.
Mignani, R.
Muleri, F.
Rapisarda, M.
Rashevsky, A.
Rea, N.
Rubini, A.
Tenzer, C.
Wilson-Hodge, C.
Winter, B.
Wood, K.
Zampa, G.
Zampa, N.
Abramowicz, M. A.
Alpar, M. A.
Altamirano, D.
Alvarez, J. M.
Amati, L.
Amoros, C.
Antonelli, L. A.
Artigue, R.
Azzarello, P.
Bachetti, M.
Baldazzi, G.
Barbera, M.
Barbieri, C.
Basa, S.
Baykal, A.
Belmont, R.
Boirin, L.
Bonvicini, V.
Burderi, L.
Bursa, M.
Cabanac, C.
Cackett, E.
Caliandro, G. A.
Casella, P.
Chaty, S.
Chenevez, J.
Coe, M. J.
Collura, A.
Corongiu, A.
Covino, S.
Cusumano, G.
D'Amico, F.
Dall'Osso, S.
De Martino, D.
De Paris, G.
Di Persio, G.
Di Salvo, T.
Done, C.
Dovciak, M.
Drago, A.
Ertan, U.
Fabiani, S.
Falanga, M.
Fender, R.
Ferrando, P.
Ferreira, D. Della Monica
Fraser, G.
Frontera, F.
Fuschino, F.
Galvez, J. L.
Gandhi, P.
Giommi, P.
Godet, O.
Gogus, E.
Goldwurm, A.
Goetz, D.
Grassi, M.
Guttridge, P.
Hakala, P.
Henri, G.
Hermsen, W.
Horak, J.
Hornstrup, A.
in't Zand, J. J. M.
Isern, J.
Kalemci, E.
Kanbach, G.
Karas, V.
Kataria, D.
Kennedy, T.
Klochkov, D.
Kluzniak, W.
Kokkotas, K.
Kreykenbohm, I.
Krolik, J.
Kuiper, L.
Kuvvetli, I.
Kylafis, N.
Lattimer, J. M.
Lazzarotto, F.
Leahy, D.
Lebrun, F.
Lin, D.
Lund, N.
Maccarone, T.
Malzac, J.
Marisaldi, M.
Martindale, A.
Mastropietro, M.
McClintock, J.
McHardy, I.
Mendez, M.
Mereghetti, S.
Miller, M. C.
Mineo, T.
Morelli, E.
Morsink, S.
Motch, C.
Motta, S.
Munoz-Darias, T.
Naletto, G.
Neustroev, V.
Nevalainen, J.
Olive, J. F.
Orio, M.
Orlandini, M.
Orleanski, P.
Ozel, F.
Pacciani, L.
Paltani, S.
Papadakis, I.
Papitto, A.
Patruno, A.
Pellizzoni, A.
Petracek, V.
Petri, J.
Petrucci, P. O.
Phlips, B.
Picolli, L.
Possenti, A.
Psaltis, D.
Rambaud, D.
Reig, P.
Remillard, R.
Rodriguez, J.
Romano, P.
Romanova, M.
Schanz, T.
Schmid, C.
Segreto, A.
Shearer, A.
Smith, A.
Smith, P. J.
Soffitta, P.
Stergioulas, N.
Stolarski, M.
Stuchlik, Z.
Tiengo, A.
Torres, D.
Toeroek, G.
Turolla, R.
Uttley, P.
Vaughan, S.
Vercellone, S.
Waters, R.
Watts, A.
Wawrzaszek, R.
Webb, N.
Wilms, J.
Zampieri, L.
Zezas, A.
Ziolkowski, J.
TI The Large Observatory for X-ray Timing (LOFT)
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Missions; X-ray timing; compact objects; black holes; neutron stars
ID SILICON DRIFT DETECTOR; BLACK-HOLE; PROPORTIONAL COUNTER; OSCILLATIONS;
ALICE; CONSTRAINTS; SUPERAGILE; DISCOVERY; BINARIES; EQUATION
AB High-time-resolution X-ray observations of compact objects provide direct access to strong-field gravity, to the equation of state of ultradense matter and to black hole masses and spins. A 10 m(2)-class instrument in combination with good spectral resolution is required to exploit the relevant diagnostics and answer two of the fundamental questions of the European Space Agency (ESA) Cosmic Vision Theme "Matter under extreme conditions", namely: does matter orbiting close to the event horizon follow the predictions of general relativity? What is the equation of state of matter in neutron stars? The Large Observatory For X-ray Timing (LOFT), selected by ESA as one of the four Cosmic Vision M3 candidate missions to undergo an assessment phase, will revolutionise the study of collapsed objects in our galaxy and of the brightest supermassive black holes in active galactic nuclei. Thanks to an innovative design and the development of large-area monolithic silicon drift detectors, the Large Area Detector (LAD) on board LOFT will achieve an effective area of similar to 12 m(2) (more than an order of magnitude larger than any spaceborne predecessor) in the 2-30 keV range (up to 50 keV in expanded mode), yet still fits a conventional platform and small/medium-class launcher. With this large area and a spectral resolution of < 260 eV, LOFT will yield unprecedented information on strongly curved spacetimes and matter under extreme conditions of pressure and magnetic field strength.
C1 [Feroci, M.; Campana, R.; Costa, E.; De Rosa, A.; Del Monte, E.; Di Cosimo, S.; Donnarumma, I.; Evangelista, Y.; Muleri, F.; Rapisarda, M.; Rubini, A.; Di Persio, G.; Fabiani, S.; Lazzarotto, F.; Mastropietro, M.; Morelli, E.; Pacciani, L.; Soffitta, P.] INAF IASF Roma, I-00133 Rome, Italy.
[Feroci, M.; Campana, R.; Del Monte, E.; Rapisarda, M.; Rubini, A.; Pacciani, L.] INFN Roma Tor Vergata, Rome, Italy.
[Stella, L.; Israel, G. L.; Antonelli, L. A.] INAF OAR, I-00040 Monte Porzio Catone, Italy.
[van der Klis, M.; Altamirano, D.; Patruno, A.; Watts, A.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands.
[Courvoisier, T. J. -L.; Bozzo, E.; Azzarello, P.; Paltani, S.] Univ Geneva, ISDC, Geneva, Switzerland.
[Hernanz, M.; Rea, N.; Altamirano, D.; Alvarez, J. M.; Caliandro, G. A.; Galvez, J. L.; Isern, J.; Torres, D.] IEEC CSIC, Barcelona, Spain.
[Hudec, R.; Petracek, V.] Czech Tech Univ, CR-16635 Prague, Czech Republic.
[Santangelo, A.; Tenzer, C.; Klochkov, D.; Kokkotas, K.; Schanz, T.] Univ Tubingen, Tubingen, Germany.
[Walton, D.; Zane, S.; Mignani, R.; Winter, B.; Guttridge, P.; Kataria, D.; Kennedy, T.; Smith, A.; Smith, P. J.] MSSL UCL, Surrey, England.
[Zdziarski, A.; Kluzniak, W.; Ziolkowski, J.] Nicholas Copernicus Astron Ctr, Warsaw, Poland.
[Barret, D.; Amoros, C.; Artigue, R.; Bachetti, M.; Belmont, R.; Cabanac, C.; Godet, O.; Lin, D.; Malzac, J.; Olive, J. F.; Rambaud, D.; Webb, N.] IRAP, Toulouse, France.
[Belloni, T.; Campana, S.; Covino, S.; Motta, S.; Munoz-Darias, T.] INAF OA Brera, Milan, Italy.
[Braga, J.; D'Amico, F.] INPE, Sao Jose Dos Campos, Brazil.
[Brandt, S.; Budtz-Jorgensen, C.; Chenevez, J.; Ferreira, D. Della Monica; Hornstrup, A.; Kuvvetli, I.; Lund, N.] DTU Space, Copenhagen, Denmark.
[den Herder, J. -W.; Haas, D.; Jonker, P.; Hermsen, W.; in't Zand, J. J. M.; Kuiper, L.; Waters, R.] SRON, Utrecht, Netherlands.
[Huovelin, J.; Korpela, S.; Nevalainen, J.] Univ Helsinki, Helsinki, Finland.
[Pohl, M.] Univ Geneva, DPNC, CH-1211 Geneva, Switzerland.
[Ray, P.; Wood, K.; Phlips, B.] NRL, Washington, DC USA.
[Vacchi, A.; Rashevsky, A.; Zampa, G.; Zampa, N.; Bonvicini, V.] Ist Nazl Fis Nucl, Trieste, Italy.
[Argan, A.; De Paris, G.] INAF Headquarters, Rome, Italy.
[Attina, P.] Thales Alenia, Turin, Italy.
[Bertuccio, G.] Politecn Milan, I-20133 Milan, Italy.
[Chakrabarty, D.; Remillard, R.] MIT, Cambridge, MA 02139 USA.
[Labanti, C.; Amati, L.; Fuschino, F.; Marisaldi, M.; Orlandini, M.] INAF IASF Bologna, Bologna, Italy.
[Malcovati, P.; Grassi, M.; Picolli, L.] Univ Pavia, I-27100 Pavia, Italy.
[Mignani, R.] Univ Zielona Gora, Inst Astron, Geneva, Poland.
[Rapisarda, M.] ENEA Frascati, Rome, Italy.
[Wilson-Hodge, C.] NASA MSFC, Huntsville, AL USA.
[Abramowicz, M. A.] Gothenburg Univ, Gothenburg, Sweden.
[Alpar, M. A.; Ertan, U.; Gogus, E.; Kalemci, E.] Sabanci Univ, Istanbul, Turkey.
[Baldazzi, G.] Ist Nazl Fis Nucl, I-40126 Bologna, Italy.
[Barbera, M.; Collura, A.; Di Salvo, T.] Univ Palermo, Palermo, Italy.
[Barbieri, C.; Naletto, G.; Turolla, R.] Univ Padua, Padua, Italy.
[Basa, S.] LAM, Marseille, France.
[Baykal, A.] Middle E Tech Univ, TR-06531 Ankara, Turkey.
[Boirin, L.; Motch, C.; Petri, J.] Observ Astron, Strasbourg, France.
[Burderi, L.] Univ Cagliari, Cagliari, Italy.
[Bursa, M.; Dovciak, M.; Horak, J.; Karas, V.] Prague Astron Inst, Prague, Czech Republic.
[Cackett, E.] Univ Cambridge, Cambridge, England.
[Casella, P.; Coe, M. J.; Fender, R.; Maccarone, T.; McHardy, I.; Uttley, P.] Univ Southampton, Southampton SO9 5NH, Hants, England.
[Chaty, S.; Ferrando, P.; Goldwurm, A.; Goetz, D.; Lebrun, F.; Rodriguez, J.] CEA Saclay, Gi Sur Yvette, France.
[Corongiu, A.; Papitto, A.; Pellizzoni, A.; Possenti, A.] INAF OA Cagliari, Cagliari, Italy.
[Cusumano, G.; Mineo, T.; Romano, P.; Segreto, A.; Vercellone, S.] INAF IASF Palermo, Palermo, Italy.
[Dall'Osso, S.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[De Martino, D.] INAF OA Capodimonte, Naples, Italy.
[Done, C.] Univ Durham, Durham, England.
[Drago, A.; Frontera, F.] Univ Ferrara, I-44100 Ferrara, Italy.
[Falanga, M.] ISSI Bern, Bern, Switzerland.
[Fraser, G.; Martindale, A.; Vaughan, S.] Univ Leicester, Leicester, Leics, England.
[Gandhi, P.] SAS JAXA, Kanagawa, Japan.
[Giommi, P.] ASI, Rome, Italy.
[Hakala, P.; Nevalainen, J.] Finnish Ctr Astron ESO, FINCA, Piikkio, Finland.
[Henri, G.; Petrucci, P. O.] Lab Astrophys Grenoble, Grenoble, France.
[Kanbach, G.] MPE, Garching, Germany.
[Kreykenbohm, I.; Schmid, C.; Wilms, J.] Univ Erlangen Nurnberg, Erlangen, Germany.
[Krolik, J.] Johns Hopkins Univ, Baltimore, MD USA.
[Kylafis, N.; Paltani, S.; Papadakis, I.; Reig, P.; Zezas, A.] Univ Crete, Iraklion, Greece.
[Lattimer, J. M.] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Leahy, D.] Univ Calgary, Calgary, AB, Canada.
[McClintock, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mendez, M.] Univ Groningen, Groningen, Netherlands.
[Mereghetti, S.; Tiengo, A.] INAF IASF Milano, Milan, Italy.
[Miller, M. C.] Univ Maryland, College Pk, MD 20742 USA.
[Morsink, S.] Univ Alberta, Edmonton, AB, Canada.
[Neustroev, V.] Oulu Univ, Oulu, Finland.
[Orio, M.] INAF OA Torino, Turin, Italy.
[Orleanski, P.; Stolarski, M.; Wawrzaszek, R.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
[Ozel, F.; Psaltis, D.] Univ Arizona, Tucson, AZ USA.
[Reig, P.] FORTH, Iraklion, Greece.
[Romanova, M.] Cornell Univ, Ithaca, NY USA.
[Shearer, A.] Galway Univ, Galway, Ireland.
[Stergioulas, N.] Aristotle Univ Thessaloniki, GR-54006 Thessaloniki, Greece.
[Stuchlik, Z.; Toeroek, G.] Silesian Univ Opava, Opava, Czech Republic.
[Torres, D.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Zampieri, L.] INAF OA Padova, Padua, Italy.
RP Feroci, M (reprint author), INAF IASF Roma, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM marco.feroci@iasf-roma.inaf.it; luigi.stella@oa-roma.inaf.it
RI Drago, Alessandro/F-6347-2012; Lazzarotto, Francesco/J-4670-2012;
Baldazzi, Giuseppe/B-4112-2011; Wilms, Joern/C-8116-2013; Kylafis,
Nikolaos/C-4555-2011; Schmid, Christian/H-9633-2013; Kreykenbohm,
Ingo/H-9659-2013; Tecnologias espaciai, Inct/I-2415-2013; Reig,
Pablo/A-1198-2014; Papadakis, Iossif/C-3235-2011; Mendez,
Mariano/C-8011-2012; Karas, Vladimir/C-1559-2013; Bursa,
Michal/G-9004-2014; Orlandini, Mauro/H-3114-2014; Horak,
Jiri/G-9015-2014; Hernanz, Margarita/K-1770-2014; Vacchi,
Andrea/C-1291-2010; Dovciak, Michal/F-4258-2014; Shearer,
Andy/N-7609-2014; Kokkotas, Kostas/B-7878-2010; Isern,
Jordi/B-1844-2015; Campana, Riccardo/F-5272-2015; Neustroev,
Vitaly/B-6351-2008; Rea, Nanda/I-2853-2015; Amati, Lorenzo/N-5586-2015;
done, chris/D-4605-2016; Ferreira, Desiree/M-1666-2016; Malcovati,
Piero/S-2458-2016; Naletto, Giampiero/S-6329-2016; Zezas,
Andreas/C-7543-2011;
OI Baldazzi, Giuseppe/0000-0002-6657-1645; Wilms,
Joern/0000-0003-2065-5410; Kylafis, Nikolaos/0000-0003-0928-0996;
Kreykenbohm, Ingo/0000-0001-7335-1803; Reig, Pablo/0000-0002-6446-3050;
Mendez, Mariano/0000-0003-2187-2708; Karas,
Vladimir/0000-0002-5760-0459; Orlandini, Mauro/0000-0003-0946-3151;
Hernanz, Margarita/0000-0002-8651-7910; Vacchi,
Andrea/0000-0003-3855-5856; Dovciak, Michal/0000-0003-0079-1239;
Shearer, Andy/0000-0001-7903-0074; Kokkotas, Kostas/0000-0001-6048-2919;
Isern, Jordi/0000-0002-0819-9574; Campana, Riccardo/0000-0002-4794-5453;
Rea, Nanda/0000-0003-2177-6388; Amati, Lorenzo/0000-0001-5355-7388;
done, chris/0000-0002-1065-7239; Ferreira, Desiree/0000-0003-4003-3256;
Malcovati, Piero/0000-0001-6514-9672; Naletto,
Giampiero/0000-0003-2007-3138; Zezas, Andreas/0000-0001-8952-676X; Di
Salvo, Tiziana/0000-0002-3220-6375; collura,
alfonso/0000-0001-9534-1235; Corongiu, Alessandro/0000-0002-5924-3141;
Israel, GianLuca/0000-0001-5480-6438; Pellizzoni, Alberto
Paolo/0000-0002-4590-0040; Campana, Sergio/0000-0001-6278-1576;
Pacciani, Luigi/0000-0001-6897-5996; Segreto,
Alberto/0000-0001-7341-6603; giommi, paolo/0000-0002-2265-5003; Mineo,
Teresa/0000-0002-4931-8445; Labanti, Claudio/0000-0002-5086-3619;
Feroci, Marco/0000-0002-7617-3421; Soffitta, Paolo/0000-0002-7781-4104;
Cusumano, Giancarlo/0000-0002-8151-1990; de Martino,
Domitilla/0000-0002-5069-4202; De Rosa, Alessandra/0000-0001-5668-6863;
Covino, Stefano/0000-0001-9078-5507; Ray, Paul/0000-0002-5297-5278;
Casella, Piergiorgio/0000-0002-0752-3301; Huovelin,
Juhani/0000-0002-6276-5776; Bachetti, Matteo/0000-0002-4576-9337;
Rodriguez, Jerome/0000-0002-4151-4468; Chaty,
Sylvain/0000-0002-5769-8601; Tiengo, Andrea/0000-0002-6038-1090;
MEREGHETTI, SANDRO/0000-0003-3259-7801; Zampieri,
Luca/0000-0002-6516-1329; Vercellone, Stefano/0000-0003-1163-1396;
Fuschino, Fabio/0000-0003-2139-3299; Lazzarotto,
Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523;
Barbera, Marco/0000-0002-3188-7420; Donnarumma,
Immacolata/0000-0002-4700-4549; Marisaldi, Martino/0000-0002-4000-3789
NR 32
TC 128
Z9 128
U1 5
U2 69
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 415
EP 444
DI 10.1007/s10686-011-9237-2
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600010
ER
PT J
AU Roques, JP
Jourdain, E
Bassani, L
Bazzano, A
Belmont, R
Bird, AJ
Caroli, E
Chauvin, M
Clark, D
Gehrels, N
Goerlach, U
Harrisson, F
Laurent, P
Malzac, J
Medina, P
Merloni, A
Paltani, S
Stephen, J
Ubertini, P
Wilms, J
AF Roques, Jean-Pierre
Jourdain, Elisabeth
Bassani, Loredana
Bazzano, Angela
Belmont, Renaud
Bird, A. J.
Caroli, E.
Chauvin, M.
Clark, D.
Gehrels, N.
Goerlach, U.
Harrisson, F.
Laurent, P.
Malzac, J.
Medina, P.
Merloni, A.
Paltani, S.
Stephen, J.
Ubertini, P.
Wilms, J.
TI PheniX: a new vision for the hard X-ray sky
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Hard X-rays; Germanium; Grazing incidence optics; Space instrument
ID ACTIVE GALACTIC NUCLEI; ACCRETING BLACK-HOLES; LOW/HARD STATE; EMISSION;
BROAD; COMPTONIZATION; BLAZARS; PULSARS; LINES; MODEL
AB We are proposing a mission devoted to high energy X-ray astronomy that is based on a focusing telescope operating in the 1-200 keV energy range but optimized for the hard X-ray range. The main scientific topics concern: Physics of compact objects: The proximity of compact objects provides a unique laboratory to study matter and radiation in extreme conditions of temperature and density in strong gravitational environment. The emission of high energy photons from these objects is far from being understood. The unprecedented sensitivity in the high energy domain will allow a precise determination of the non-thermal processes at work in the vicinity of compact objects. The full 1-200 keV energy coverage will be ideal to disentangle the emission processes produced in the spacetime regions most affected by strong-gravity, as well as the physical links: disk-thermal emission-iron line-comptonisation-reflection-non-thermal emission-jets. Neutron stars-magnetic field-cyclotron lines: Time resolved spectroscopy (and polarimetry) at ultra-high sensitivity of AXP, milliseconds pulsars and magnetars will give new tools to study the role of the synchrotron processes at work in these objects. Cyclotron lines-direct measurement of magnetic filed-equation of state constraints-short bursts-giant flares could all be studied with great details. AGN: The large sensitivity improvement will provide detailed spectral properties of the high energy emission of AGN's. This will give a fresh look to the connection between accretion and jet emission and will provide a new understanding of the physical processes at work. Detection of high-redshift active nuclei in this energy range will allow to introduce an evolutionary aspect to high-energy studies of AGN, probing directly the origin of the Cosmic X-ray Background also in the non-thermal range (> 20 keV). Element formation-Supernovae: The energy resolution achievable for this mission (< 0.5 keV) and a large high energy effective area are ideally suited for the 44Ti line study (68 and 78 keV). This radioactive nuclei emission will give an estimate of their quantities and speed in their environment. In addition the study of the spatial structure and spectral emission of SNR will advance our knowledge of the dynamics of supernovae explosions, of particles acceleration mechanisms and how the elements are released in the interstellar medium. Instrumental design: The progress of X-ray focusing optics techniques allows a major step in the instrumental design: the collecting area becomes independent of the detection area. This drastically reduces the instrumental background and will open a new era. The optics will be based on depth-graded multi-layer mirrors in a Wolter I configuration. To obtain a significant effective area in the hundred of keV range a focal length in the 40-50 meters range (attainable with a deployable mast) is needed. In addition such a mission could benefit from recent progress made on mirror coating. We propose to cover the 1-200 keV energy range with a single detector, a double-sided Germanium strip detector operating at 80 K. The main features will be: (a) good energy resolution (.150 keV at 5 keV and <.5 keV at 100 keV), (b) 3 dimensional event localization with a low number of electronic chains, (c) background rejection by the 3D localization, (d) polarisation capabilities in the Compton regime.
C1 [Roques, Jean-Pierre; Jourdain, Elisabeth; Belmont, Renaud; Chauvin, M.; Clark, D.; Malzac, J.] Univ Toulouse, CNRS, IRAP, F-31028 Toulouse 4, France.
[Bassani, Loredana; Caroli, E.; Stephen, J.] INAF IASF Bologna, CNR, Ist Astrofis Spaziale & Fis Cosm, Area Ric, I-40129 Bologna, Italy.
[Bazzano, Angela; Ubertini, P.] INAF, IASF, Sez Roma, IT-00133 Rome, Italy.
[Bird, A. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Laurent, P.] Lab Astroparticule & Cosmol, F-75205 Paris 13, France.
[Laurent, P.] IFU Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Merloni, A.] TUM, Max Planck Inst Extraterr Phys, Excellence Cluster Universe, D-85748 Garching, Germany.
[Paltani, S.] Observ Geneva, INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Wilms, J.] Univ Erlangen Nurnberg, D-91054 Erlangen, Germany.
[Goerlach, U.; Medina, P.] Inst Pluridisciplinaire Hubert Curien, F-67037 Strasbourg 2, France.
[Harrisson, F.] 290 17 Caltech, Space Radiat Lab, Pasadena, CA 91125 USA.
RP Roques, JP (reprint author), Univ Toulouse, CNRS, IRAP, 9 Ave Colonel Roche,BP44346, F-31028 Toulouse 4, France.
EM roques@cesr.fr
RI Wilms, Joern/C-8116-2013; laurent, philippe/E-6211-2013; Caroli,
Ezio/G-1427-2012;
OI Wilms, Joern/0000-0003-2065-5410; Caroli, Ezio/0000-0001-8468-7433;
Bassani, Loredana/0000-0003-4858-6963
NR 34
TC 8
Z9 8
U1 1
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 489
EP 517
DI 10.1007/s10686-011-9236-3
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600013
ER
PT J
AU den Herder, JW
Piro, L
Ohashi, T
Kouveliotou, C
Hartmann, DH
Kaastra, JS
Amati, L
Andersen, MI
Arnaud, M
Atteia, JL
Bandler, S
Barbera, M
Barcons, X
Barthelmy, S
Basa, S
Basso, S
Boer, M
Branchini, E
Branduardi-Raymont, G
Borgani, S
Boyarsky, A
Brunetti, G
Budtz-Jorgensen, C
Burrows, D
Butler, N
Campana, S
Caroli, E
Ceballos, M
Christensen, F
Churazov, E
Comastri, A
Colasanti, L
Cole, R
Content, R
Corsi, A
Costantini, E
Conconi, P
Cusumano, G
de Plaa, J
De Rosa, A
Del Santo, M
Di Cosimo, S
De Pasquale, M
Doriese, R
Ettori, S
Evans, P
Ezoe, Y
Ferrari, L
Finger, H
Figueroa-Feliciano, T
Friedrich, P
Fujimoto, R
Furuzawa, A
Fynbo, J
Gatti, F
Galeazzi, M
Gehrels, N
Gendre, B
Ghirlanda, G
Ghisellini, G
Gilfanov, M
Giommi, P
Girardi, M
Grindlay, J
Cocchi, M
Godet, O
Guedel, M
Haardt, F
den Hartog, R
Hepburn, I
Hermsen, W
Hjorth, J
Hoekstra, H
Holland, A
Hornstrup, A
van der Horst, A
Hoshino, A
in't Zand, J
Irwin, K
Ishisaki, Y
Jonker, P
Kitayama, T
Kawahara, H
Kawai, N
Kelley, R
Kilbourne, C
de Korte, P
Kusenko, A
Kuvvetli, I
Labanti, M
Macculi, C
Maiolino, R
Hesse, MM
Matsushita, K
Mazzotta, P
McCammon, D
Mendez, M
Mignani, R
Mineo, T
Mitsuda, K
Mushotzky, R
Molendi, S
Moscardini, L
Natalucci, L
Nicastro, F
O'Brien, P
Osborne, J
Paerels, F
Page, M
Paltani, S
Pedersen, K
Perinati, E
Ponman, T
Pointecouteau, E
Predehl, P
Porter, S
Rasmussen, A
Rauw, G
Rottgering, H
Roncarelli, M
Rosati, P
Quadrini, E
Ruchayskiy, O
Salvaterra, R
Sasaki, S
Sato, K
Savaglio, S
Schaye, J
Sciortino, S
Shaposhnikov, M
Sharples, R
Shinozaki, K
Spiga, D
Sunyaev, R
Suto, Y
Takei, Y
Tanvir, N
Tashiro, M
Tamura, T
Tawara, Y
Troja, E
Tsujimoto, M
Tsuru, T
Ubertini, P
Ullom, J
Ursino, E
Verbunt, F
van de Voort, F
Viel, M
Wachter, S
Watson, D
Weisskopf, M
Werner, N
White, N
Willingale, R
Wijers, R
Yamasaki, N
Yoshikawa, K
Zane, S
AF den Herder, Jan-Willem
Piro, Luigi
Ohashi, Takaya
Kouveliotou, Chryssa
Hartmann, Dieter H.
Kaastra, Jelle S.
Amati, L.
Andersen, M. I.
Arnaud, M.
Atteia, J. -L.
Bandler, S.
Barbera, M.
Barcons, X.
Barthelmy, S.
Basa, S.
Basso, S.
Boer, M.
Branchini, E.
Branduardi-Raymont, G.
Borgani, S.
Boyarsky, A.
Brunetti, G.
Budtz-Jorgensen, C.
Burrows, D.
Butler, N.
Campana, S.
Caroli, E.
Ceballos, M.
Christensen, F.
Churazov, E.
Comastri, A.
Colasanti, L.
Cole, R.
Content, R.
Corsi, A.
Costantini, E.
Conconi, P.
Cusumano, G.
de Plaa, J.
De Rosa, A.
Del Santo, M.
Di Cosimo, S.
De Pasquale, M.
Doriese, R.
Ettori, S.
Evans, P.
Ezoe, Y.
Ferrari, L.
Finger, H.
Figueroa-Feliciano, T.
Friedrich, P.
Fujimoto, R.
Furuzawa, A.
Fynbo, J.
Gatti, F.
Galeazzi, M.
Gehrels, N.
Gendre, B.
Ghirlanda, G.
Ghisellini, G.
Gilfanov, M.
Giommi, P.
Girardi, M.
Grindlay, J.
Cocchi, M.
Godet, O.
Guedel, M.
Haardt, F.
den Hartog, R.
Hepburn, I.
Hermsen, W.
Hjorth, J.
Hoekstra, H.
Holland, A.
Hornstrup, A.
van der Horst, A.
Hoshino, A.
in't Zand, J.
Irwin, K.
Ishisaki, Y.
Jonker, P.
Kitayama, T.
Kawahara, H.
Kawai, N.
Kelley, R.
Kilbourne, C.
de Korte, P.
Kusenko, A.
Kuvvetli, I.
Labanti, M.
Macculi, C.
Maiolino, R.
Mas Hesse, M.
Matsushita, K.
Mazzotta, P.
McCammon, D.
Mendez, M.
Mignani, R.
Mineo, T.
Mitsuda, K.
Mushotzky, R.
Molendi, S.
Moscardini, L.
Natalucci, L.
Nicastro, F.
O'Brien, P.
Osborne, J.
Paerels, F.
Page, M.
Paltani, S.
Pedersen, K.
Perinati, E.
Ponman, T.
Pointecouteau, E.
Predehl, P.
Porter, S.
Rasmussen, A.
Rauw, G.
Rottgering, H.
Roncarelli, M.
Rosati, P.
Quadrini, E.
Ruchayskiy, O.
Salvaterra, R.
Sasaki, S.
Sato, K.
Savaglio, S.
Schaye, J.
Sciortino, S.
Shaposhnikov, M.
Sharples, R.
Shinozaki, K.
Spiga, D.
Sunyaev, R.
Suto, Y.
Takei, Y.
Tanvir, N.
Tashiro, M.
Tamura, T.
Tawara, Y.
Troja, E.
Tsujimoto, M.
Tsuru, T.
Ubertini, P.
Ullom, J.
Ursino, E.
Verbunt, F.
van de Voort, F.
Viel, M.
Wachter, S.
Watson, D.
Weisskopf, M.
Werner, N.
White, N.
Willingale, R.
Wijers, R.
Yamasaki, N.
Yoshikawa, K.
Zane, S.
TI ORIGIN: metal creation and evolution from the cosmic dawn
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE X-ray; Mission; Gamma-ray bursts; Clusters of galaxies; Warm-hot
intergalactic medium; Chemical evolution
ID GAMMA-RAY BURSTS; HOT INTERGALACTIC MEDIUM; ABSORPTION-SPECTRA;
NUCLEOSYNTHESIS; REDSHIFT; GALAXIES; CLUSTERS; UNIVERSE; FOREST; YIELDS
AB ORIGIN is a proposal for the M3 mission call of ESA aimed at the study of metal creation from the epoch of cosmic dawn. Using high-spectral resolution in the soft X-ray band, ORIGIN will be able to identify the physical conditions of all abundant elements between C and Ni to red-shifts of z = 10, and beyond. The mission will answer questions such as: When were the first metals created? How does the cosmic metal content evolve? Where do most of the metals reside in the Universe? What is the role of metals in structure formation and evolution? To reach out to the early Universe ORIGIN will use Gamma-Ray Bursts (GRBs) to study their local environments in their host galaxies. This requires the capability to slew the satellite in less than a minute to the GRB location. By studying the chemical composition and properties of clusters of galaxies we can extend the range of exploration to lower redshifts (z similar to 0.2). For this task we need a high-resolution spectral imaging instrument with a large field of view. Using the same instrument, we can also study the so far only partially detected baryons in the Warm-Hot Intergalactic Medium (WHIM). The less dense part of the WHIM will be studied using absorption lines at low redshift in the spectra for GRBs. The ORIGIN mission includes a Transient Event Detector (coded mask with a sensitivity of 0.4 photon/cm(2)/s in 10 s in the 5-150 keV band) to identify and localize 2000 GRBs over a five year mission, of which similar to 65 GRBs have a redshift > 7. The Cryogenic Imaging Spectrometer, with a spectral resolution of 2.5 eV, a field of view of 30 arcmin and large effective area below 1 keV has the sensitivity to study clusters up to a significant fraction of the virial radius and to map the denser parts of the WHIM (factor 30 higher than achievable with current instruments). The payload is complemented by a Burst InfraRed Telescope to enable onboard red-shift determination of GRBs (hence securing proper follow up of high-z bursts) and also probes the mildly ionized state of the gas. Fast repointing is achieved by a dedicated Controlled Momentum Gyro and a low background is achieved by the selected low Earth orbit.
C1 [den Herder, Jan-Willem; Kaastra, Jelle S.; Costantini, E.; de Plaa, J.; den Hartog, R.; Hermsen, W.; in't Zand, J.; Jonker, P.; de Korte, P.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Piro, Luigi; Colasanti, L.; Corsi, A.; De Rosa, A.; Del Santo, M.; Di Cosimo, S.; Gendre, B.; Cocchi, M.; Macculi, C.; Natalucci, L.; Ubertini, P.] INAF Ist Astrofis Spaziale & Fis Cosm, Rome, Italy.
[Ohashi, Takaya; Ezoe, Y.; Ishisaki, Y.; Kawahara, H.; Sasaki, S.] Tokyo Metropolitan Univ, Tokyo 158, Japan.
[Kouveliotou, Chryssa; van der Horst, A.; Weisskopf, M.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Hartmann, Dieter H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Amati, L.; Caroli, E.; Labanti, M.] INAF Ist Astrofis Spaziale & Fis Cosm, Bologna, Italy.
[Andersen, M. I.; Fynbo, J.; Hjorth, J.; Pedersen, K.; Watson, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Arnaud, M.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Atteia, J. -L.] Observ Midi Pyrenees, LAT, F-31400 Toulouse, France.
[Bandler, S.; Barthelmy, S.; Gehrels, N.; Kelley, R.; Kilbourne, C.; Porter, S.; Troja, E.; White, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Barbera, M.; Cusumano, G.; Mineo, T.; Perinati, E.; Sciortino, S.] INAF Ist Astrofis Spaziale, Palermo, Italy.
[Barcons, X.; Ceballos, M.] IFCA, Santander, Spain.
[Basa, S.] Observ Marseille, F-13248 Marseille, France.
[Basso, S.; Campana, S.; Conconi, P.; Ghirlanda, G.; Ghisellini, G.; Spiga, D.] Osservatorio Astronomico Brera, INAF, Milan, Italy.
[Boer, M.] Observ Haute Provence, Haute Provence, France.
[Branchini, E.; Ursino, E.] Univ Roma III, Rome, Italy.
[Branduardi-Raymont, G.; Cole, R.; De Pasquale, M.; Hepburn, I.; Mignani, R.; Page, M.; Zane, S.] UCL, Mullard Space Sci Lab, London, England.
[Borgani, S.] INAF Osservatorio Astron, Trieste, Italy.
[Boyarsky, A.] CERN, Geneva, Switzerland.
[Brunetti, G.] INAF IRA, Bologna, Italy.
[Budtz-Jorgensen, C.; Christensen, F.; Hornstrup, A.; Kuvvetli, I.] Tech Univ Denmark, DNSC, Copenhagen, Denmark.
[Burrows, D.] Penn State Univ, Philadelphia, PA USA.
[Butler, N.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Churazov, E.; Gilfanov, M.; Sunyaev, R.] Max Planck Inst Astrophys, Munich, Germany.
[Costantini, E.; Ettori, S.; Moscardini, L.] INAF Osservatorio Astron, Bologna, Italy.
[Content, R.; Sharples, R.] Univ Durham, Durham, England.
[Doriese, R.; Irwin, K.; Ullom, J.] NIST, Boulder, CO USA.
[Evans, P.; O'Brien, P.; Osborne, J.; Tanvir, N.; Willingale, R.] Univ Leicester, Leicester, Leics, England.
[Ferrari, L.; Gatti, F.] Ist Nazl Fis Nucl, I-16146 Genoa, Italy.
[Finger, H.] Univ Space Res Assoc, Huntsvile, AL USA.
[Figueroa-Feliciano, T.] MIT, Cambridge, MA 02139 USA.
[Friedrich, P.; Predehl, P.; Savaglio, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Fujimoto, R.; Hoshino, A.] Kanazawa Univ, Kanazawa, Ishikawa, Japan.
[Furuzawa, A.; Tawara, Y.] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
[Galeazzi, M.] Univ Miami, Coral Gables, FL 33124 USA.
[Giommi, P.] ASI Data Ctr, Frascati, Italy.
[Grindlay, J.] Harvard Univ, CfA, Cambridge, MA 02138 USA.
[Godet, O.; Pointecouteau, E.] CESR, Toulouse, France.
[Guedel, M.] Univ Vienna, Vienna, Austria.
[Haardt, F.; Salvaterra, R.] Univ Insubria, Como, Italy.
[Hoekstra, H.; Rottgering, H.; Schaye, J.; van de Voort, F.] Leiden Univ, Leiden, Netherlands.
[Holland, A.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Kitayama, T.] Toho Univ, Chiba 2748510, Japan.
[Kawai, N.] Tokyo Inst Technol, Tokyo 152, Japan.
[Kusenko, A.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Maiolino, R.; Nicastro, F.] INAF Osservatorio Astron Roma, Rome, Italy.
[Mas Hesse, M.] Ctr Astrobiol CSIC INTA, Madrid, Spain.
[Matsushita, K.; Sato, K.] Tokyo Univ Sci, Tokyo 162, Japan.
[Mazzotta, P.] Univ Roma Tor Vergata, Rome, Italy.
[McCammon, D.] Univ Wisconsin, Madison, WI USA.
[Mendez, M.] Univ Groningen, Groningen, Netherlands.
[Mitsuda, K.; Takei, Y.; Tamura, T.; Tsujimoto, M.; Yamasaki, N.] JAXA, Inst Space & Astronaut Sci, Kanagawa, Japan.
[Mushotzky, R.] Univ Maryland, College Pk, MD 20742 USA.
[Molendi, S.; Quadrini, E.] INAF Ist Astrofis Spaziale & Fis Cosm, Milan, Italy.
[Paerels, F.] Columbia Univ, Columbia, NY USA.
[Paltani, S.] Univ Geneva, ISDC, Versoix, Switzerland.
[Ponman, T.] Univ Birmingham, Birmingham, W Midlands, England.
[Rasmussen, A.; Werner, N.] KIPAC Stanford, Palo Alto, CA USA.
[Rauw, G.] Univ Liege, Liege, Belgium.
[Roncarelli, M.] Univ Bologna, Bologna, Italy.
[Rosati, P.] ESO, Garching, Germany.
[Ruchayskiy, O.; Shaposhnikov, M.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Shinozaki, K.] JAXA, Aerosp Res & Dev Directorate, Ibaraki, Japan.
[Suto, Y.] Univ Tokyo, Tokyo, Japan.
[Tashiro, M.] Saitama Univ, Saitama 3388570, Japan.
[Tsuru, T.] Kyoto Univ, Kyoto, Japan.
[Verbunt, F.] Univ Utrecht, Utrecht, Netherlands.
[Wachter, S.] CALTECH, Pasadena, CA 91125 USA.
[Wijers, R.] Univ Amsterdam, Amsterdam, Netherlands.
[Yoshikawa, K.] Univ Tsukuba, Ibaraki, Japan.
RP den Herder, JW (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
EM J.W.A.den.Herder@sron.nl
RI Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Guedel,
Manuel/C-8486-2015; Ruchayskiy, Oleg/E-3698-2015; Watson,
Darach/E-4521-2015; Caroli, Ezio/G-1427-2012; Ettori,
Stefano/N-5004-2015; Amati, Lorenzo/N-5586-2015; Comastri,
Andrea/O-9543-2015; Ceballos, Maria Teresa/K-9140-2014; Mazzotta,
Pasquale/B-1225-2016; Gatti, Flavio/K-4568-2013; Tashiro,
Makoto/J-4562-2012; Kelley, Richard/K-4474-2012; Tamura,
Takayuki/K-8236-2012; Churazov, Eugene/A-7783-2013; Yamasaki,
Noriko/C-2252-2008; Bandler, Simon/A-6258-2010; Sharples,
Ray/N-7309-2013; gendre, bruce/O-2923-2013; Mendez, Mariano/C-8011-2012;
PIRO, LUIGI/E-4954-2013; Mitsuda, Kazuhisa/C-2649-2008; Barcons,
Xavier/L-3335-2014;
OI Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306;
Guedel, Manuel/0000-0001-9818-0588; Ruchayskiy,
Oleg/0000-0001-8073-3068; Watson, Darach/0000-0002-4465-8264; Caroli,
Ezio/0000-0001-8468-7433; Ettori, Stefano/0000-0003-4117-8617; Amati,
Lorenzo/0000-0001-5355-7388; Comastri, Andrea/0000-0003-3451-9970;
Ceballos, Maria Teresa/0000-0001-6074-3621; Mazzotta,
Pasquale/0000-0002-5411-1748; Spiga, Daniele/0000-0003-1163-7843; Del
Santo, Melania/0000-0002-1793-1050; Mineo, Teresa/0000-0002-4931-8445;
Cusumano, Giancarlo/0000-0002-8151-1990; Nicastro,
Fabrizio/0000-0002-6896-1364; Campana, Sergio/0000-0001-6278-1576;
giommi, paolo/0000-0002-2265-5003; Viel, Matteo/0000-0002-2642-5707;
Wijers, Ralph/0000-0002-3101-1808; Bandler, Simon/0000-0002-5112-8106;
Sharples, Ray/0000-0003-3449-8583; gendre, bruce/0000-0002-9077-2025;
Mendez, Mariano/0000-0003-2187-2708; PIRO, LUIGI/0000-0003-4159-3984;
Barcons, Xavier/0000-0003-1081-8861; De Rosa,
Alessandra/0000-0001-5668-6863; Molendi, Silvano/0000-0002-2483-278X;
Schaye, Joop/0000-0002-0668-5560; Savaglio, Sandra/0000-0003-2354-3238;
Ghirlanda, Giancarlo/0000-0001-5876-9259; Ghisellini,
Gabriele/0000-0002-0037-1974; Barbera, Marco/0000-0002-3188-7420;
Macculi, Claudio/0000-0002-7887-1485; Branchini,
Enzo/0000-0002-0808-6908; Borgani, Stefano/0000-0001-6151-6439;
Salvaterra, Ruben/0000-0002-9393-8078
FU Astrium UK
FX The team likes to express its appreciation for the support of Astrium UK
for the present study. Earlier studies, which also confirmed the
feasibility of this concept were carried out by Thales/Alenia and
NASA/MSFC.
NR 36
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U1 0
U2 22
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD OCT
PY 2012
VL 34
IS 2
SI SI
BP 519
EP 549
DI 10.1007/s10686-011-9224-7
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012IU
UT WOS:000309230600014
ER
PT J
AU Kandula, M
AF Kandula, M.
TI Frost growth and densification on a flat surface in laminar flow with
variable humidity
SO INTERNATIONAL COMMUNICATIONS IN HEAT AND MASS TRANSFER
LA English
DT Article
DE Frost growth; Densification; Variable humidity; Flat surface; Laminar
flow
ID THERMAL-CONDUCTIVITY; ATMOSPHERIC AIR; COLD PLATE; PARAMETERS
AB Experiments are performed concerning frost growth and densification in laminar flow over a flat surface under conditions of constant and variable humidity. The flat plate test specimen is made of aluminum-6031, and has dimensions of 0.3 m x 0.3 m x 6.35 mm. Results for the first variable humidity case are obtained for a plate temperature of 255.4 K, air velocity of 1.77 m/s, air temperature of 295.1 K, and a relative humidity continuously ranging from 81 to 54%. The second variable humidity test case corresponds to plate temperature of 255.4 K, air velocity of 2.44 m/s, air temperature of 291.8 K, and a relative humidity ranging from 66 to 59%. Results for the constant humidity case are obtained for a plate temperature of 263.7 K, air velocity of 1.7 m/s, air temperature of 295 K, and a relative humidity of 71.6%. Comparisons of the data with the author's frost model extended to accommodate variable humidity suggest satisfactory agreement between the theory and the data for both constant and variable humidity. (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
FU NASA Kennedy Space Center
FX The author would like to thank Brian Hunter and Kevin Jumper at the
Cryogenics Laboratory at NASA Kennedy Space Center with regard to
experimental test support. This work was funded by NASA Kennedy Space
Center, with Mark Collard as Project Manager. Thanks are also due to
Stanley Starr (Chief, Applied Physics Branch) of NASA Kennedy Space
Center for review and helpful suggestions. Papers by the author from
1973-1982 were published with the name K. Mastanaiah.
NR 14
TC 4
Z9 6
U1 1
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0735-1933
J9 INT COMMUN HEAT MASS
JI Int. Commun. Heat Mass Transf.
PD OCT
PY 2012
VL 39
IS 8
BP 1030
EP 1034
DI 10.1016/j.icheatmasstransfer.2012.07.016
PG 5
WC Thermodynamics; Mechanics
SC Thermodynamics; Mechanics
GA 011EJ
UT WOS:000309147200003
ER
PT J
AU Hurst, TP
Munch, SB
Lavelle, KA
AF Hurst, Thomas P.
Munch, Stephan B.
Lavelle, Kate A.
TI Thermal reaction norms for growth vary among cohorts of Pacific cod
(Gadus macrocephalus)
SO MARINE BIOLOGY
LA English
DT Article
ID NORTHERN ROCK SOLE; PLAICE PLEURONECTES-PLATESSA; DEPENDENT SEX
DETERMINATION; EARLY-LIFE-HISTORY; ATLANTIC COD; VERTEBRAL NUMBER;
CLIMATE-CHANGE; EVOLUTIONARY SIGNIFICANCE; LEPIDOPSETTA-POLYXYSTRA;
COMPENSATORY GROWTH
AB While much effort has been directed at determining the spatial scales of adaptation in thermal reaction norms for growth, it is widely assumed that these reaction norms have high temporal stability. Water temperatures in the Gulf of Alaska in 2007 were the coldest on record since the mid-1970s and we present evidence that the thermal reaction norm for growth of age-0 Pacific cod (Gadus macrocephalus) in this cohort differed significantly from two adjacent cohorts. In addition to exhibiting higher growth potential at low temperatures, the 2007 cohort had a higher mean vertebral count, consistent with the widespread thermal effect known as "Jordan's Rule." Variation among cohorts in these physiological and morphological traits suggests a persistent response to environmental history (epigenetic effect). Temperature-induced phenotypic plasticity in the reaction norm for growth has significant implications for using growth rates to evaluate habitat quality and illustrates the complex responses of fishes to climate variability.
C1 [Hurst, Thomas P.] Natl Ocean & Atmospher Adm, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
[Munch, Stephan B.] NOAA, Fisheries Ecol Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Santa Cruz, CA 95060 USA.
[Lavelle, Kate A.] Oregon State Univ, Hatfield Marine Sci Ctr, Newport, OR 97365 USA.
RP Hurst, TP (reprint author), Natl Ocean & Atmospher Adm, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 S Marine Sci Dr, Newport, OR 97365 USA.
EM thomas.hurst@noaa.gov; steve.munch@noaa.gov; kate.a.lavelle@gmail.com
RI Hurst, Thomas/N-1401-2013
FU National Science Foundation [OCE-0648515]; North Pacific Research Board
[R0605]
FX The authors thank T. Tripp, M. Spencer, B. Knoth, and B. Laurel for
assistance with fish collection and shipping. Staff in the
AFSC-Fisheries Behavioral Ecology Program including S. Haines, M.
Ottmar, P. Iseri assisted with growth experiments. Assistance with
X-rays was provided by D. Simon and D. Markle. This manuscript
benefitted from discussions with C. Schreck. B. Laurel, A. Stoner, J.
Miller, and two anonymous reviewers provided valuable comments on this
manuscript. K. A. L. was supported by a National Science Foundation
Research Experience for Undergraduates internship under award
OCE-0648515 to the Hatfield Marine Science Center of Oregon State
University. This work was also supported in part by a grant from the
North Pacific Research Board (#R0605 to B. Laurel et al.). This is
publication #353 of the North Pacific Research Board. 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. Reference to trade names does not imply endorsement by the
National Marine Fisheries Service.
NR 73
TC 4
Z9 4
U1 1
U2 33
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0025-3162
J9 MAR BIOL
JI Mar. Biol.
PD OCT
PY 2012
VL 159
IS 10
BP 2173
EP 2183
DI 10.1007/s00227-012-2003-9
PG 11
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 010OM
UT WOS:000309103900006
ER
PT J
AU Ottmar, ML
Hurst, TP
AF Ottmar, Michele L.
Hurst, Thomas P.
TI Thermal effects on swimming activity and habitat choice in juvenile
Pacific cod (Gadus macrocephalus)
SO MARINE BIOLOGY
LA English
DT Article
ID POLLOCK THERAGRA-CHALCOGRAMMA; WALLEYE POLLOCK; ATLANTIC COD;
BERING-SEA; LABORATORY CONDITIONS; POECILIA-RETICULATA; LOCOMOTOR
CAPACITY; ACTIVITY PATTERNS; TEMPERATURE; BEHAVIOR
AB The behavioral responses of fishes to temperature variation have received less attention than physiological responses, despite their direct implications for predator-prey dynamics in aquatic ecosystems. In this paper, we describe the temperature dependence of swimming performance and behavioral characteristics of juvenile Pacific cod (Gadus macrocephalus; 75-125 mm total length). Maximum swimming speeds increased with temperature and body size. Routine swimming speeds of Pacific cod in small groups of similarly sized fish (N = 6) increased with body size and were 34 % faster at 9 A degrees C than at 2 A degrees C. The response to temperature was opposite that previously described for juvenile walleye pollock (Theragra chalcogramma), reflecting species-specific differences in behavioral responses. In a separate experiment, we demonstrated the effect of temperature on habitat selection of juvenile Pacific cod: Use of an artificial eelgrass patch in a 5-m-long laboratory tank was significantly greater at 9 A degrees C than at 2 A degrees C. These results illustrate that temperature affects a range of behavioral traits that play important roles in determining the frequency and outcomes of predator-prey interactions.
C1 [Ottmar, Michele L.; Hurst, Thomas P.] Natl Ocean & Atmospher Adm, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
RP Hurst, TP (reprint author), Natl Ocean & Atmospher Adm, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 S Marine Sci Dr, Newport, OR 97365 USA.
EM thomas.hurst@noaa.gov
RI Hurst, Thomas/N-1401-2013
NR 61
TC 4
Z9 4
U1 4
U2 27
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0025-3162
EI 1432-1793
J9 MAR BIOL
JI Mar. Biol.
PD OCT
PY 2012
VL 159
IS 10
BP 2185
EP 2194
DI 10.1007/s00227-012-2004-8
PG 10
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 010OM
UT WOS:000309103900007
ER
PT J
AU Behrangi, A
Kubar, T
Lambrigtsen, B
AF Behrangi, Ali
Kubar, Terry
Lambrigtsen, Bjorn
TI Phenomenological Description of Tropical Clouds Using CloudSat Cloud
Classification
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; RADIATION BUDGET EXPERIMENT; LIQUID WATER PATH;
1998 EL-NINO; BOUNDARY-LAYER; MICROPHYSICAL PROPERTIES;
STATISTICAL-ANALYSES; SEASONAL-VARIATION; DIURNAL-VARIATIONS; DEEP
CONVECTION
AB Two years of tropical oceanic cloud observations are analyzed using the operational CloudSat cloud classification product and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CA LIPSO) lidar. Relationships are examined between cloud types, sea surface temperature (SST), and location during the Cloud Sat early morning and afternoon overpasses. Based on Cloud Sat and combined lidar radar products, the maximum and minimum cloud fractions occur at SSTs near 303 and 299 K, respectively, corresponding to deep convective/detrained cloud populations and the transition from shallow to deep convection. For SSTs below approximately 301 K, low clouds (stratiform and stratocumulus) are dominant (cloud fraction between 0.15 and 0.37) whereas high clouds are dominant for SSTs greater than about 301 K (cloud fraction between 0.18 and 0.28). Consistent with previous studies, most tropical low clouds are associated with lower SSTs, with a strong inverse linear relationship between low cloud frequency and SST. For all cloud types except nimbostratus, stratus, and stratocumulus, a sharp increase in frequency of occurrence is observed for SSTs between 299 and 300.5 K, deduced as the onset of deeper convection. Peak fractions of high, deep convective, altostratus, and altocumulus clouds occur at SSTs close to 303 K, while cumulus clouds, which have lower tops, show a smooth cloud fractional peak about 2 degrees cooler. Deep convective and other high cloud types decrease sharply above SSTs of 303 K, in accordance with previous work suggesting a narrow window of tropical deep convection. Finally, significant cloud frequency differences exist between CloudSat early morning and afternoon overpasses, suggesting a diurnal cycle of some cloud types, particularly stratocumulus, high, and deep convective clouds.
C1 [Behrangi, Ali; Kubar, Terry; Lambrigtsen, Bjorn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-300, Pasadena, CA 91109 USA.
EM ali.behrangi@jpl.nasa.gov
NR 63
TC 10
Z9 10
U1 3
U2 25
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD OCT
PY 2012
VL 140
IS 10
BP 3235
EP 3249
DI 10.1175/MW12-D-11-00247.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 013PQ
UT WOS:000309317700007
ER
PT J
AU Vallisneri, M
AF Vallisneri, Michele
TI Testing general relativity with gravitational waves: A reality check
SO PHYSICAL REVIEW D
LA English
DT Article
ID INSPIRALLING COMPACT BINARIES; PARAMETERS; GRAVITY; LISA; MASS
AB The observations of gravitational-wave signals from astrophysical sources such as binary inspirals will be used to test general relativity for self-consistency and against alternative theories of gravity. I describe a simple formula that can be used to characterize the prospects of such tests, by estimating the matched-filtering signal-to-noise ratio required to detect non-general-relativistic corrections of a given magnitude. The formula is valid for sufficiently strong signals; it requires the computation of a single number, the fitting factor between the general-relativistic and corrected waveform families; and it can be applied to all tests that embed general relativity in a larger theory, including tests of individual theories such as Brans-Dicke gravity, as well as the phenomenological schemes that introduce corrections and extra terms in the post-Newtonian phasing expressions of inspiral waveforms. The formula suggests that the volume-limited gravitational-wave searches performed with second-generation ground-based detectors would detect alternative-gravity corrections to general-relativistic waveforms no smaller than 1%-10% (corresponding to fitting factors of 0.9 to 0.99).
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vallisneri, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU LISA Mission Science Office; JPL RTD program
FX I am grateful to Walter Del Pozzo, Marc Favata, Ilya Mandel, Chris
Messenger, Reinhard Prix, and (especially) Curt Cutler, Nico Yunes, and
the anonymous PRD referee for useful discussions and suggestions. This
work was supported by the LISA Mission Science Office and by the JPL RTD
program, and it was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.
NR 45
TC 15
Z9 15
U1 1
U2 1
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 OCT 1
PY 2012
VL 86
IS 8
DI 10.1103/PhysRevD.86.082001
PG 7
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 014AL
UT WOS:000309347300001
ER
PT J
AU Chen, KS
Serpico, SB
Smith, JA
AF Chen, Kun-Shan
Serpico, Sebastiano B.
Smith, James A.
TI Remote Sensing of Natural Disasters
SO PROCEEDINGS OF THE IEEE
LA English
DT Editorial Material
C1 [Chen, Kun-Shan] Natl Cent Univ, Ctr Space & Remote Sensing Res, Tao Yuan, Taiwan.
[Chen, Kun-Shan] Natl Cent Univ, Commun Syst Res Ctr, Tao Yuan, Taiwan.
[Serpico, Sebastiano B.] Univ Genoa, Fac Engn, I-16126 Genoa, Italy.
[Serpico, Sebastiano B.] Univ Genoa, Signal Proc & Telecommun Lab, Dept Biophys & Elect Engn, I-16126 Genoa, Italy.
[Smith, James A.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
RP Chen, KS (reprint author), Natl Cent Univ, Ctr Space & Remote Sensing Res, Tao Yuan, Taiwan.
NR 0
TC 3
Z9 3
U1 2
U2 18
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9219
J9 P IEEE
JI Proc. IEEE
PD OCT
PY 2012
VL 100
IS 10
SI SI
BP 2794
EP 2797
DI 10.1109/JPROC.2012.2205835
PG 4
WC Engineering, Electrical & Electronic
SC Engineering
GA 008ZX
UT WOS:000308996200002
ER
PT J
AU Duda, KA
Abrams, M
AF Duda, Kenneth A.
Abrams, Michael
TI ASTER Satellite Observations for International Disaster Management
SO PROCEEDINGS OF THE IEEE
LA English
DT Article
DE ASTER; disaster; emergency response; International Charter; natural
hazards; satellite remote sensing
ID SPACEBORNE THERMAL EMISSION; REFLECTION RADIOMETER ASTER; MAJOR
DISASTERS; NATURAL HAZARDS; CHARTER; EARTHQUAKE
AB When lives are threatened or lost due to catastrophic disasters, and when massive financial impacts are experienced, international emergency response teams rapidly mobilize to provide urgently required support. Satellite observations of affected areas often provide essential insight into the magnitude and details of the impacts. The large cost and high complexity of developing and operating satellite flight and ground systems encourages international collaboration in acquiring imagery for such significant global events in order to speed delivery of critical information to help those affected, and optimize spectral, spatial, and temporal coverage of the areas of interest. The International Charter-Space and Major Disasters was established to enable such collaboration in sensor tasking during times of crisis and is often activated in response to calls for assistance from authorized users. Insight is provided from a U. S. perspective into sensor support for Charter activations and other disaster events through a description of the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER), which has been used to support emergency situations for over a decade through its expedited tasking and near real-time data delivery capabilities. Examples of successes achieved and challenges encountered in international collaboration to develop related systems and fulfill tasking requests suggest operational considerations for new missions as well as areas for future enhancements.
C1 [Duda, Kenneth A.] SGT, Greenbelt, MD 20770 USA.
[Duda, Kenneth A.] NASA, Land Proc Distributed Act Arch Ctr, Sioux Falls, SD 57198 USA.
[Abrams, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Duda, KA (reprint author), SGT, Greenbelt, MD 20770 USA.
EM duda@usgs.gov; Michael.J.Abrams@jpl.nasa.gov
FU U.S. Geological Survey [G10PC00044]
FX Manuscript received July 29, 2011; revised November 22, 2011 and March
6, 2012; accepted March 7, 2012. Date of publication May 18, 2012; date
of current version September 14, 2012. The work of K. A. Duda was
performed under U.S. Geological Survey Contract G10PC00044. The work of
M. Abrams was performed at the Jet Propulsion Laboratory/California
Institute of Technology under contract to the National Aeronautics and
Space Administration.
NR 49
TC 3
Z9 3
U1 1
U2 17
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9219
J9 P IEEE
JI Proc. IEEE
PD OCT
PY 2012
VL 100
IS 10
SI SI
BP 2798
EP 2811
DI 10.1109/JPROC.2012.2191929
PG 14
WC Engineering, Electrical & Electronic
SC Engineering
GA 008ZX
UT WOS:000308996200003
ER
PT J
AU Anyamba, A
Linthicum, KJ
Small, J
Britch, SC
Tucker, CJ
AF Anyamba, Assaf
Linthicum, Kenneth J.
Small, Jennifer
Britch, Seth C.
Tucker, Compton J.
TI Remote Sensing Contributions to Prediction and Risk Assessment of
Natural Disasters Caused by Large-Scale Rift Valley Fever Outbreaks
SO PROCEEDINGS OF THE IEEE
LA English
DT Article
DE Arthropod-borne virus; climate variability; El Nino/Southern Oscillation
(ENSO); normalized difference vegetation index; predictive model; Rift
Valley fever virus (RVFV); risk management and mitigation
ID NINO SOUTHERN-OSCILLATION; HANTAVIRUS PULMONARY SYNDROME; EL-NINO;
VEGETATION INDEX; EAST-AFRICA; ECOLOGICAL CONDITIONS; RAINFALL
VARIABILITY; CLIMATE VARIABILITY; SATELLITE DATA; UNITED-STATES
AB Remotely sensed vegetation measurements for the last 30 years combined with other climate data sets such as rainfall and sea surface temperatures have come to play an important role in the study of the ecology of arthropod-borne diseases. We show that epidemics and epizootics of previously unpredictable Rift Valley fever (RVF) are directly influenced by large-scale flooding associated with the El Nino/Southern Oscillation (ENSO). This flooding affects the ecology of disease transmitting arthropod vectors through vegetation development and other bioclimatic factors. This information is now utilized to monitor, model, and map areas of potential RVF outbreaks and is used as an early warning system for risk reduction of outbreaks to human and animal health, trade, and associated economic impacts. The continuation of such satellite measurements is critical to anticipating, preventing, and managing disease epidemics and epizootics and other climate-related disasters.
C1 [Anyamba, Assaf] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
[Linthicum, Kenneth J.; Britch, Seth C.] ARS, Ctr Med Agr & Vet Entomol, USDA, Gainesville, FL 32608 USA.
RP Anyamba, A (reprint author), NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
EM assaf.anyamba@nasa.gov; kenneth.linthicum@ars.usda.gov;
jennifer.l.small@nasa.gov; seth.britch@ars.usda.gov;
compton.j.tucker@nasa.gov
FU U.S. Department of Defense; Armed Forces Health Surveillance Center;
Division of GEIS Operations; U.S. Department of Agriculture;
Agricultural Research Service; National Aeronautics and Space
Administration
FX Manuscript received September 21, 2011; revised March 9, 2012; accepted
March 20, 2012. Date of publication June 14, 2012; date of current
version September 14, 2012. This work was supported in part by the U.S.
Department of Defense, Armed Forces Health Surveillance Center, Division
of GEIS Operations, the U.S. Department of Agriculture, Agricultural
Research Service, and National Aeronautics and Space Administration.
NR 54
TC 1
Z9 1
U1 4
U2 30
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9219
EI 1558-2256
J9 P IEEE
JI Proc. IEEE
PD OCT
PY 2012
VL 100
IS 10
SI SI
BP 2824
EP 2834
DI 10.1109/JPROC.2012.2194469
PG 11
WC Engineering, Electrical & Electronic
SC Engineering
GA 008ZX
UT WOS:000308996200005
ER
PT J
AU Karaca, HE
Acar, E
Basaran, B
Noebe, RD
Bigelow, G
Garg, A
Yang, F
Mills, MJ
Chumlyakov, YI
AF Karaca, H. E.
Acar, E.
Basaran, B.
Noebe, R. D.
Bigelow, G.
Garg, A.
Yang, F.
Mills, M. J.
Chumlyakov, Y. I.
TI Effects of aging on [111] oriented NiTiHfPd single crystals under
compression
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Shape memory alloys (SMA), Phase transformation; Damping; Ageing; High
strength shape memory alloys
ID SHAPE-MEMORY ALLOYS; NI; BEHAVIOR; TRANSFORMATION
AB The effects of aging on the shape memory properties of [1 1 1] oriented Ni45.3Ti29.7Hf20Pd5 single crystals were investigated under compression. Thermal cycling under stress and superelasticity experiments were conducted after 3 h aging at 550 and 600 degrees C and were found to be dependent on aging condition. Reversible strain of up to 2.2% and a work output of 33 J cm(-3) were possible at an ultra-high stress level of 1500 MPa. (c) 2012 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Karaca, H. E.; Acar, E.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Basaran, B.] Univ Houston, Dept Engn Technol, Houston, TX 77004 USA.
[Noebe, R. D.; Bigelow, G.; Garg, A.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Yang, F.; Mills, M. J.] Ohio State Univ, Dept Mat Sci, Columbus, OH 43210 USA.
[Chumlyakov, Y. I.] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia.
RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM karaca@engr.uky.edu
RI yuriy, chumlyakov/C-6033-2009; Mills, Michael/I-6413-2013; Chumlyakov,
Yuriy/R-6496-2016
FU NASA Fundamental Aeronautics Program under the Supersonics Project; Dale
Hopkins; API; NASA EPSCOR program [NNX11AQ31A]; NASA Kentucky EPSCoR
program [NNX10A-V39A]; Kentucky Statewide EPSCoR; RFBR Project
[10-03-00154a]
FX This work was supported in part by the NASA Fundamental Aeronautics
Program under the Supersonics Project, Dale Hopkins, API, the NASA
EPSCOR program under Grant No. NNX11AQ31A, NASA Kentucky EPSCoR program
under Grant No. NNX10A-V39A, Kentucky Statewide EPSCoR and RFBR Project
with Grant No. 10-03-00154a.
NR 18
TC 21
Z9 23
U1 3
U2 17
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6462
J9 SCRIPTA MATER
JI Scr. Mater.
PD OCT
PY 2012
VL 67
IS 7-8
BP 728
EP 731
DI 10.1016/j.scriptamat.2012.06.028
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 010LS
UT WOS:000309096500026
ER
PT J
AU Raffa, V
Riggio, C
Smith, MW
Jordan, KC
Cao, W
Cuschieri, A
AF Raffa, V.
Riggio, C.
Smith, M. W.
Jordan, K. C.
Cao, W.
Cuschieri, A.
TI BNNT-Mediated Irreversible Electroporation: Its Potential on Cancer
Cells
SO TECHNOLOGY IN CANCER RESEARCH & TREATMENT
LA English
DT Article
DE Boron nitride nanotubes; Irreversible electroporation
ID BORON-NITRIDE NANOTUBES; ABLATION TECHNIQUE; CARBON NANOTUBES; TISSUE
ABLATION; IN-VITRO; CYTOCOMPATIBILITY; TUMORS; DELIVERY; DEATH
AB Irreversible lethal electroporation (IRE) is a new non-thermal ablation modality that uses short pulses of high amplitude static electric fields (up 1000V/cm) to create irreversible pores in the cell membrane, thus, causing cell death. Recently, IRE has emerged as a promising clinical modality for cancer disease treatment. Here, we investigated the responses of tumour human He La cells when subjected to IRE in the presence of BNNTs. These consist of tiny tubes of B and N atoms (arranged in hexagons) with diameters ranging from a 1 to 3 nanometres and lengths <2 mu m. BNNTs have attracted wide attention because of their unique electrical properties. We speculate that BNNTs, when interacting with cells exposed to static electrical fields, amplify locally the electric field, leading to cell death. In this work, electroporation assays were performed with a commercial electroporator using the cell-specific protocol suggested by the supplier (exponential decay wave, time constant 20ms) with the specific aim to compare IRE in absence and in presence of BNNTs. We observed that BNNTs have the capacity to decrease substantially the voltage required for IRE. When cells were pulsed at 800V/cm, we observed a 2,2-fold reduction in cell survival in the presence of BNNTs compared to controls. We conclude that the death of the tumour cells exposed to IRE is strongly enhanced in the presence of BNNTs, indicating their potential therapeutic application.
C1 [Raffa, V.; Riggio, C.; Cuschieri, A.] Scuola Super Sant Anna, Inst Life Sci, Pisa, Italy.
[Raffa, V.] Univ Pisa, Dept Biol, Pisa, Italy.
[Smith, M. W.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Jordan, K. C.] Jefferson Natl Accelerator Facil, Jefferson Lab, Newport News, VA USA.
[Cao, W.] Old Dominion Univ, Newport News, VA USA.
RP Raffa, V (reprint author), Scuola Super Sant Anna, Inst Life Sci, Pisa, Italy.
EM v.raffa@sssup.it
RI Cuschieri, Alfred/A-7634-2013;
OI RAFFA, VITTORIA/0000-0002-4289-9937
FU Magnetic Nanoparticle for Nerve Regeneration NanoSci-E+2008 project;
NanoDiab-1 project
FX Authors thank Mr. Mauro Muracchini from Meckgroup for his support in
cell counting assay. This work was partially supported by the Magnetic
Nanoparticle for Nerve Regeneration NanoSci-E+2008 project, cofounded by
European Commission (EC)/Consiglio Nazionale delle Ricerche (CNR), and
by the NanoDiab-1 project cofounded by Fondazione Cassa di Risparmio di
Pisa.
NR 37
TC 16
Z9 16
U1 1
U2 10
PU ADENINE PRESS
PI SCHENECTADY
PA 2066 CENTRAL AVE, SCHENECTADY, NY 12304 USA
SN 1533-0346
J9 TECHNOL CANCER RES T
JI Technol. Cancer Res. Treat.
PD OCT
PY 2012
VL 11
IS 5
BP 459
EP 465
DI 10.7785/tcrt.2012.500258
PG 7
WC Oncology
SC Oncology
GA 006YI
UT WOS:000308855300007
PM 22475064
ER
PT J
AU Shuping, RY
Vacca, WD
Kassis, M
Yu, KC
AF Shuping, R. Y.
Vacca, William D.
Kassis, Marc
Yu, Ka Chun
TI SPECTRAL CLASSIFICATION OF THE BRIGHTEST OBJECTS IN THE GALACTIC
STAR-FORMING REGION W40
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars; ISM: individual objects (W40);
stars: early-type; stars: pre-main sequence
ID INFRARED TELESCOPE FACILITY; HERBIG AE/BE STARS; CIRCUMSTELLAR DISKS;
STELLAR PARAMETERS; AQUILA RIFT; GM-AURIGAE; OB STARS; B-STARS;
SEQUENCE; ATLAS
AB We present high signal-to-noise, moderate resolution (R approximate to 2000) near-infrared spectra, as well as 10 mu m imaging, for the brightest members of the central stellar cluster in the W40 H-II region, obtained using the SpeX and MIRSI instruments at NASA's Infrared Telescope Facility. Using these observations combined with archival Spitzer Space Telescope data, we have determined the spectral classifications, extinction, distances, and spectral energy distributions (SEDs) for the brightest members of the cluster. Of the eight objects observed, we identify four main-sequence (MS) OB stars (one late-O, three early-B), two Herbig Ae/Be stars, and two low-mass young stellar objects (Class II). Strong He (I) absorption at 1.083 mu m in the MS star spectra strongly suggests that at least some of these sources are in fact close binaries. Two out of the four MS stars also show significant infrared excesses typical of circumstellar disks. Extinctions and distances were determined for each MS star by fitting model stellar atmospheres to the SEDs. We estimate a distance to the cluster of between 455 and 535 pc, which agrees well with earlier (but far less precise) distance estimates. We conclude that the late-O star we identify is the dominant source of Lyman continuum luminosity needed to power the W40 H-II region and is the likely source of the stellar wind that has blown a large (approximate to 4 pc) pinched-waist bubble observed in wide-field mid-IR images. We also suggest that 3.6 cm radio emission observed from some of the sources in the cluster is likely not due to emission from ultracompact H-II regions, as suggested in other work, due to size constraints based on our derived distance to the cluster. Finally, we also present a discussion of the curious source IRS 3A, which has a very strong mid-IR excess (despite its B3 MS classification) and appears to be embedded in a dusty envelope roughly 2700 AU in size.
C1 [Shuping, R. Y.] Space Sci Inst, Boulder, CO USA.
[Shuping, R. Y.; Vacca, William D.] NASA, Univ Space Res Assoc, Stratospher Observ Infrared Astron, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kassis, Marc] WM Keck Observ, Kamuela, HI 96743 USA.
[Yu, Ka Chun] Denver Museum Nat & Sci, Denver, CO 80205 USA.
RP Shuping, RY (reprint author), NASA, Univ Space Res Assoc, Stratospher Observ Infrared Astron, Ames Res Ctr, MS 211-3, Moffett Field, CA 94035 USA.
EM rshuping@spacescience.org
FU Universities Space Research Assoc. (USRA) [209000771]; University of
Hawaii under Cooperative Agreement with the National Aeronautics and
Space Administration, Science Mission Directorate, Planetary Astronomy
Program [NNX-08AE38A]
FX This research has been supported in part by the Universities Space
Research Assoc. (USRA) under contract 209000771 to R. Y. Shuping at the
Space Science Institute. Data were obtained at the Infrared Telescope
Facility, which is operated by the University of Hawaii under
Cooperative Agreement NNX-08AE38A with the National Aeronautics and
Space Administration, Science Mission Directorate, Planetary Astronomy
Program. This work is based in part on observations made with the
Spitzer Space Telescope, and data obtained from the NASA/IPAC Infrared
Science Archive, both of which are operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with the
National Aeronautics and Space Administration.
NR 49
TC 10
Z9 10
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 OCT
PY 2012
VL 144
IS 4
AR 116
DI 10.1088/0004-6256/144/4/116
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 007WO
UT WOS:000308919300026
ER
PT J
AU Axelsson, M
Baldini, L
Barbiellini, G
Baring, MG
Bellazzini, R
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Caliandro, GA
Cameron, RA
Caraveo, PA
Cecchi, C
Chaves, RCG
Chekhtman, A
Chiang, J
Claus, R
Conrad, J
Cutini, S
D'Ammando, F
de Palma, F
Dermer, CD
Silva, EDE
Drell, PS
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fukazawa, Y
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giroletti, M
Godfrey, G
Guiriec, S
Hadasch, D
Hanabata, Y
Hayashida, M
Hou, X
Iyyani, S
Jackson, MS
Kocevski, D
Kuss, M
Larsson, J
Larsson, S
Longo, F
Loparco, F
Lundman, C
Mazziotta, MN
McEnery, JE
Mizuno, T
Monzani, ME
Moretti, E
Morselli, A
Murgia, S
Nuss, E
Nymark, T
Ohno, M
Omodei, N
Pesce-Rollins, M
Piron, F
Pivato, G
Racusin, JL
Raino, S
Razzano, M
Razzaque, S
Reimer, A
Roth, M
Ryde, F
Sanchez, DA
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Stamatikos, M
Tibaldo, L
Tinivella, M
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Winer, BL
Wood, KS
Burgess, JM
Bhat, PN
Bissaldi, E
Briggs, MS
Connaughton, V
Fishman, G
Fitzpatrick, G
Foley, S
Gruber, D
Kippen, RM
Kouveliotou, C
Jenke, P
McBreen, S
McGlynn, S
Meegan, C
Paciesas, WS
Pelassa, V
Preece, R
Tierney, D
von Kienlin, A
Wilson-Hodge, C
Xiong, S
Pe'er, A
AF Axelsson, M.
Baldini, L.
Barbiellini, G.
Baring, M. G.
Bellazzini, R.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Cecchi, C.
Chaves, R. C. G.
Chekhtman, A.
Chiang, J.
Claus, R.
Conrad, J.
Cutini, S.
D'Ammando, F.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Drell, P. S.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giroletti, M.
Godfrey, G.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Hayashida, M.
Hou, X.
Iyyani, S.
Jackson, M. S.
Kocevski, D.
Kuss, M.
Larsson, J.
Larsson, S.
Longo, F.
Loparco, F.
Lundman, C.
Mazziotta, M. N.
McEnery, J. E.
Mizuno, T.
Monzani, M. E.
Moretti, E.
Morselli, A.
Murgia, S.
Nuss, E.
Nymark, T.
Ohno, M.
Omodei, N.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Racusin, J. L.
Raino, S.
Razzano, M.
Razzaque, S.
Reimer, A.
Roth, M.
Ryde, F.
Sanchez, D. A.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Stamatikos, M.
Tibaldo, L.
Tinivella, M.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Winer, B. L.
Wood, K. S.
Burgess, J. M.
Bhat, P. N.
Bissaldi, E.
Briggs, M. S.
Connaughton, V.
Fishman, G.
Fitzpatrick, G.
Foley, S.
Gruber, D.
Kippen, R. M.
Kouveliotou, C.
Jenke, P.
McBreen, S.
McGlynn, S.
Meegan, C.
Paciesas, W. S.
Pelassa, V.
Preece, R.
Tierney, D.
von Kienlin, A.
Wilson-Hodge, C.
Xiong, S.
Pe'er, A.
TI GRB110721A: AN EXTREME PEAK ENERGY AND SIGNATURES OF THE PHOTOSPHERE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst: individual (GRB110721A);
radiation mechanisms: thermal
ID GAMMA-RAY-BURSTS; NONTHERMAL EMISSION; SPECTRAL COMPONENT; PROMPT
EMISSION; GRB090902B; MONITOR; PULSES
AB GRB110721A was observed by the Fermi Gamma-ray Space Telescope using its two instruments, the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM). The burst consisted of one major emission episode which lasted for similar to 24.5 s (in the GBM) and had a peak flux of (5.7 +/- 0.2) x 10(-5) erg s(-1) cm(-2). The time-resolved emission spectrum is best modeled with a combination of a Band function and a blackbody spectrum. The peak energy of the Band component was initially 15 +/- 2 MeV, which is the highest value ever detected in a GRB. This measurement was made possible by combining GBM/BGO data with LAT Low Energy events to achieve continuous 10-100 MeV coverage. The peak energy later decreased as a power law in time with an index of -1.89 +/- 0.10. The temperature of the blackbody component also decreased, starting from similar to 80 keV, and the decay showed a significant break after similar to 2 s. The spectrum provides strong constraints on the standard synchrotron model, indicating that alternative mechanisms may give rise to the emission at these energies.
C1 [Axelsson, M.; Iyyani, S.; Jackson, M. S.; Lundman, C.; Moretti, E.; Nymark, T.; Ryde, F.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Larsson, J.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Conrad, J.; Iyyani, S.; Jackson, M. S.; Larsson, J.; Larsson, S.; Lundman, C.; Moretti, E.; Nymark, T.; Ryde, F.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[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.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.] IN2P3, CNRS, Ecole Polytech, Lab Leprince Ringuet, Palaiseau, France.
[Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Godfrey, G.; Hayashida, M.; Kocevski, D.; Monzani, M. E.; Murgia, S.; Omodei, N.; Reimer, A.; Usher, T. L.; 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.
[Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Godfrey, G.; Hayashida, M.; Kocevski, D.; Monzani, M. E.; Murgia, S.; Omodei, N.; Reimer, A.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cecchi, C.; D'Ammando, F.; Germani, S.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Germani, S.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chaves, R. C. G.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Conrad, J.; Iyyani, S.; Larsson, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy.
[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.; Racusin, J. L.; Stamatikos, M.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Ferrara, E. C.; Gehrels, N.; Guiriec, S.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Hanabata, Y.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.; Jenke, P.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hou, X.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mizuno, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France.
[Ohno, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Pivato, G.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Razzano, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Razzano, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Reimer, A.; Bissaldi, E.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Bissaldi, E.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stamatikos, M.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Burgess, J. M.; Bhat, P. N.; Briggs, M. S.; Connaughton, V.; Pelassa, V.; Preece, R.; Xiong, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Fishman, G.; Kouveliotou, C.; Jenke, P.; Wilson-Hodge, C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Fitzpatrick, G.; Foley, S.; McBreen, S.; Tierney, D.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Foley, S.; Gruber, D.; McBreen, S.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[McGlynn, S.] Tech Univ Munich, D-85748 Garching, Germany.
[Meegan, C.; Paciesas, W. S.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Pe'er, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Axelsson, M (reprint author), Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
EM magnusa@astro.su.se; josefin.larsson@astro.su.se;
moretti@particle.kth.se; felix@particle.kth.se; james.m.burgess@nasa.gov
RI Bissaldi, Elisabetta/K-7911-2016; Iyyani, Shabnam/D-8736-2017; Kuss,
Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Morselli,
Aldo/G-6769-2011; Racusin, Judith/D-2935-2012; Loparco,
Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016;
OI Sgro', Carmelo/0000-0001-5676-6214; Burgess, James/0000-0003-3345-9515;
Omodei, Nicola/0000-0002-5448-7577; /0000-0003-0065-2933; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785;
Giroletti, Marcello/0000-0002-8657-8852; Moretti,
Elena/0000-0001-5477-9097; Cutini, Sara/0000-0002-1271-2924; Gasparrini,
Dario/0000-0002-5064-9495; Bissaldi, Elisabetta/0000-0001-9935-8106;
Iyyani, Shabnam/0000-0002-2525-3464; Preece, Robert/0000-0003-1626-7335;
Caraveo, Patrizia/0000-0003-2478-8018; giglietto,
nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Loparco,
Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395;
Mazziotta, Mario /0000-0001-9325-4672; Baldini, Luca/0000-0002-9785-7726
FU K. A. Wallenberg Foundation; NASA, United States; DOE, United States;
CEA/Irfu, France; IN2P3/CNRS, France; ASI, Italy; INFN, Italy; MEXT,
Japan; KEK, Japan; JAXA, Japan; K. A. Wallenberg Foundation, Sweden;
Swedish Research Council, Sweden [623-2009-691]; SNSB, Sweden; BMWi/DLR
in Germany; Carl Tryggers Stiftelse for Vetenskaplig Forskning
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; The Fermi LAT Collaboration
acknowledges support from a number of agencies and institutes for both
development and the operation of the LAT as well as scientific data
analysis. These include NASA and DOE in the United States, CEA/Irfu and
IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in
Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council
(623-2009-691), and the SNSB in Sweden. Additional support from INAF in
Italy and CNES in France for science analysis during the operations
phase is also gratefully acknowledged. The Fermi GBM Collaboration
acknowledges support for GBM development, operations, and data analysis
from NASA in the US and BMWi/DLR in Germany. E. M. is supported by Carl
Tryggers Stiftelse for Vetenskaplig Forskning.
NR 26
TC 69
Z9 70
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 1
PY 2012
VL 757
IS 2
AR L31
DI 10.1088/2041-8205/757/2/L31
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 007XM
UT WOS:000308921700012
ER
PT J
AU Sun, XJ
Shen, SH
Leptoukh, GG
Wang, PX
Di, LP
Lu, MY
AF Sun, Xiaojuan
Shen, Suhung
Leptoukh, Gregory G.
Wang, Panxing
Di, Liping
Lu, Mingyue
TI Development of a Web-based visualization platform for climate research
using Google Earth
SO COMPUTERS & GEOSCIENCES
LA English
DT Article
DE Data visualization; KML; Google Earth; Climate study; Data sharing
AB Recently, it has become easier to access climate data from satellites, ground measurements, and models from various data centers. However, searching, accessing, and processing heterogeneous data from different sources are very time-consuming tasks. There is lack of a comprehensive visual platform to acquire distributed and heterogeneous scientific data and to render processed images from a single accessing point for climate studies. This paper documents the design and implementation of a Web-based visual, interoperable, and scalable platform that is able to access climatological fields from models, satellites, and ground stations from a number of data sources using Google Earth (GE) as a common graphical interface. The development is based on the TCP/IP protocol and various data sharing open sources, such as OPeNDAP, GDS, Web Processing Service (WPS), and Web Mapping Service (WMS). The visualization capability of integrating various measurements into GE extends dramatically the awareness and visibility of scientific results. Using embedded geographic information in the GE, the designed system improves our understanding of the relationships of different elements in a four-dimensional domain. The system enables easy and convenient synergistic research on a virtual platform for professionals and the general public, greatly advancing global data sharing and scientific research collaboration. (c) 2011 Elsevier Ltd. All rights reserved.
C1 [Sun, Xiaojuan; Wang, Panxing; Lu, Mingyue] Nanjing Univ Informat Sci & Technol, China Inst Mfg Dev, Nanjing 210044, Jiangsu, Peoples R China.
[Shen, Suhung; Di, Liping] George Mason Univ, CSISS, Fairfax, VA 22030 USA.
[Shen, Suhung; Leptoukh, Gregory G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sun, Xiaojuan] Nanjing Univ Informat Sci & Technol, Key Lab Meteorol Disaster, Minist Educ, Nanjing 210044, Jiangsu, Peoples R China.
RP Sun, XJ (reprint author), Nanjing Univ Informat Sci & Technol, China Inst Mfg Dev, 219 Ningliu Rd, Nanjing 210044, Jiangsu, Peoples R China.
EM sxjzy709@nuist.edu.cn
FU NASA ROSES program [NNH08ZDA001N-LCLUC]; National Natural Science
Foundation of China [40901244]; Social Commonwealth Research Program of
the Ministry of Science and Technology, China [GYHY200806009]; Graduate
Innovation project of Jiangsu Province, China [CX10B_288Z]
FX This work is supported by NASA ROSES 2008 program (NNH08ZDA001N-LCLUC),
National Natural Science Foundation of China (40901244), Social
Commonwealth Research Program of the Ministry of Science and Technology,
China (GYHY200806009) and Graduate Innovation project of Jiangsu
Province, China (CX10B_288Z). The authors are grateful to Yueqi Bai,
Aijun Chen, and Aiguo Han at GMU CSSIS for their technique support and
valuable comments during the system development.
NR 17
TC 15
Z9 15
U1 1
U2 19
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD OCT
PY 2012
VL 47
BP 160
EP 168
DI 10.1016/j.cageo.2011.09.010
PG 9
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 002FO
UT WOS:000308517700016
ER
PT J
AU Menking, KM
Peteet, DM
Anderson, RY
AF Menking, Kirsten M.
Peteet, Dorothy M.
Anderson, Roger Y.
TI Late-glacial and Holocene vegetation and climate variability, including
major droughts, in the Sky Lakes region of southeastern New York State
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Drought; Shawangunk Mountains; Holocene; Pollen; Macrofossils; Stable
isotopes
ID NORTHEASTERN UNITED-STATES; EASTERN NORTH-AMERICA; SOUTHERN NEW-ENGLAND;
ATMOSPHERIC CIRCULATION; HUDSON HIGHLANDS; MOISTURE-BALANCE; HEMLOCK
DECLINE; LONG-TERM; USA; HISTORY
AB Sediment cores from Lakes Minnewaska and Mohonk in the Shawangunk Mountains of southeastern New York were analyzed for pollen, plant macrofossils, macroscopic charcoal, organic carbon content, carbon isotopic composition, carbon/nitrogen ratio, and lithologic changes to determine the vegetation and landscape history of the greater Catskill Mountain region since deglaciation. Pollen stratigraphy generally matches the New England pollen zones identified by Deevey (1939) and Davis (1969), with boreal genera (Picea, Abies) present during the late Pleistocene yielding to a mixed Pinus, Quercus and Tsuga forest in the early Holocene. Lake Minnewaska sediments record the Younger Dryas and possibly the 8.2 cal kyr BP climatic events in pollen and sediment chemistry along with an similar to 1400 cal yr interval of wet conditions (increasing Tsuga and declining Quercus) centered about 6400 cal yr BP. Both Minnewaska and Mohonk reveal a protracted drought interval in the middle Holocene, similar to 5700-4100 cal yr BP, during which Pinus rigida colonized the watershed, lake levels fell, and frequent fires led to enhanced hillslope erosion. Together, the records show at least three wet-dry cycles throughout the Holocene and both similarities and differences to climate records in New England and central New York. Drought intervals raise concerns for water resources in the New York City metropolitan area and may reflect a combination of enhanced La Nina, negative phase NAO, and positive phase PNA climatic patterns and/or northward shifts of storm tracks. (c) 2012 Elsevier B.V. All rights reserved.
C1 [Menking, Kirsten M.] Vassar Coll, Dept Earth Sci & Geog, Poughkeepsie, NY 12604 USA.
[Peteet, Dorothy M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Peteet, Dorothy M.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Anderson, Roger Y.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
RP Menking, KM (reprint author), Vassar Coll, Dept Earth Sci & Geog, Box 59,124 Raymond Ave, Poughkeepsie, NY 12604 USA.
EM kimenking@vassar.edu; Peteet@ldeo.columbia.edu; ryand@unm.edu
FU Priscilla Bullitt Collins Faculty Environmental Research fund at Vassar
College
FX We wish to thank Paul Huth and John Thompson of Mohonk Preserve, the
Smiley family of Mohonk Mountain House, and Tom Cobb and Haddy
Langsford, formerly of Minnewaska State Park, for providing us access to
the study areas. Andrew Schmidt, China Kreiker Mabee, Stephanie Andrews,
Beth Feingold, Sarah Pittiglio, Jeff Werner, Josh Dorin, Chuck Bolduc,
Justin Minder, Krysia Skorko, Brian Lee, and Joel Dashnaw assisted in
the coring operations. Rebecca Drury, Eric Langhans, Bevin Collins, and
Eric Snyder assisted with sample preparation. Conversations with Guy
Robinson and Andrea Lini were helpful in shaping our ideas. Funding for
radiocarbon dates and stable isotope analyses came from the Priscilla
Bullitt Collins Faculty Environmental Research fund at Vassar College.
The comments of anonymous reviewers improved the text. We thank them for
their careful attention to our work.
NR 87
TC 6
Z9 7
U1 5
U2 46
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
EI 1872-616X
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD OCT 1
PY 2012
VL 353
BP 45
EP 59
DI 10.1016/j.palaeo.2012.06.033
PG 15
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA 007OJ
UT WOS:000308897700005
ER
PT J
AU Liu, TS
Burner, AW
Jones, TW
Barrows, DA
AF Liu, Tianshu
Burner, Alpheus W.
Jones, Thomas W.
Barrows, Danny A.
TI Photogrammetric techniques for aerospace applications
SO PROGRESS IN AEROSPACE SCIENCES
LA English
DT Review
DE Photogrammetry; Optical measurements; Wind tunnel; Space structure;
Flight testing
ID PARTICLE IMAGE VELOCIMETRY; WIND-TUNNEL; MODEL DEFORMATION; ACCURACY;
VIDEOGRAMMETRY; CALIBRATION; DYNAMICS; FLOWS
AB Photogrammetric techniques have been used for measuring the important physical quantities in both ground and flight testing including aeroelastic deformation, attitude, position, shape and dynamics of objects such as wind tunnel models, flight vehicles, rotating blades and large space structures. The distinct advantage of photogrammetric measurement is that it is a non-contact, global measurement technique. Although the general principles of photogrammetry are well known particularly in topographic and aerial survey, photogrammetric techniques require special adaptation for aerospace applications. This review provides a comprehensive and systematic summary of photogrammetric techniques for aerospace applications based on diverse sources. It is useful mainly for aerospace engineers who want to use photogrammetric techniques, but it also gives a general introduction for photogrammetrists and computer vision scientists to new applications. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Liu, Tianshu] Western Michigan Univ, Dept Mech & Aeronaut Engn, Kalamazoo, MI 49008 USA.
[Burner, Alpheus W.] Jacobs Technol NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Jones, Thomas W.; Barrows, Danny A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Liu, TS (reprint author), Western Michigan Univ, Dept Mech & Aeronaut Engn, Kalamazoo, MI 49008 USA.
EM tianshu.liu@wmich.edu
NR 111
TC 14
Z9 18
U1 2
U2 35
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0376-0421
J9 PROG AEROSP SCI
JI Prog. Aeosp. Sci.
PD OCT
PY 2012
VL 54
BP 1
EP 58
DI 10.1016/j.paerosci.2012.03.002
PG 58
WC Engineering, Aerospace
SC Engineering
GA 006XP
UT WOS:000308853400001
ER
PT J
AU Rittenhouse, CD
Pidgeon, AM
Albright, TP
Culbert, PD
Clayton, MK
Flather, CH
Masek, JG
Radeloff, VC
AF Rittenhouse, Chadwick D.
Pidgeon, Anna M.
Albright, Thomas P.
Culbert, Patrick D.
Clayton, Murray K.
Flather, Curtis H.
Masek, Jeffrey G.
Radeloff, Volker C.
TI Land-Cover Change and Avian Diversity in the Conterminous United States
SO CONSERVATION BIOLOGY
LA English
DT Article
DE abundance; biodiversity; conservation; land-cover change; North American
Breeding Bird Survey; richness; abundancia; biodiversidad; cambio de
cobertura de suelo; conservacion; North American Breeding Bird Survey;
riqueza
ID BIRDS; BIODIVERSITY; LANDSCAPES; PATTERNS
AB Changes in land use and land cover have affected and will continue to affect biological diversity worldwide. Yet, understanding the spatially extensive effects of land-cover change has been challenging because data that are consistent over space and time are lacking. We used the U.S. National Land Cover Dataset Land Cover Change Retrofit Product and North American Breeding Bird Survey data to examine land-cover change and its associations with diversity of birds with principally terrestrial life cycles (landbirds) in the conterminous United States. We used mixed-effects models and model selection to rank associations by ecoregion. Land cover in 3.22% of the area considered in our analyses changed from 1992 to 2001, and changes in species richness and abundance of birds were strongly associated with land-cover changes. Changes in species richness and abundance were primarily associated with changes in nondominant types of land cover, yet in many ecoregions different types of land cover were associated with species richness than were associated with abundance. Conversion of natural land cover to anthropogenic land cover was more strongly associated with changes in bird species richness and abundance than persistence of natural land cover in nearly all ecoregions and different covariates were most strongly associated with species richness than with abundance in 11 of 17 ecoregions. Loss of grassland and shrubland affected bird species richness and abundance in forested ecoregions. Loss of wetland was associated with bird abundance in forested ecoregions. Our findings highlight the value of understanding changes in nondominant land cover types and their association with bird diversity in the United States.
C1 [Rittenhouse, Chadwick D.; Pidgeon, Anna M.; Albright, Thomas P.; Culbert, Patrick D.; Radeloff, Volker C.] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA.
[Albright, Thomas P.] Univ Nevada, Dept Geog, Lab Conservat Biogeog, Reno, NV 89557 USA.
[Albright, Thomas P.] Univ Nevada, Program Ecol Evolut & Conservat Biol, Reno, NV 89557 USA.
[Clayton, Murray K.] Univ Wisconsin, Dept Stat, Madison, WI 53706 USA.
[Flather, Curtis H.] US Forest Serv, USDA, Rocky Mt Res Stn, Ft Collins, CO 80526 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rittenhouse, CD (reprint author), Univ Connecticut, Dept Nat Resources & Environm, Unit 4087, 1376 Storrs Rd, Storrs, CT 06269 USA.
EM chadwick.rittenhouse@uconn.edu
RI Masek, Jeffrey/D-7673-2012; Radeloff, Volker/B-6124-2016; Flather,
Curtis/G-3577-2012
OI Radeloff, Volker/0000-0001-9004-221X; Flather,
Curtis/0000-0002-0623-3126
FU National Aeronautics and Space Administration (NASA); NASA; National
Science Foundation [EPS-0814372]
FX We thank the BBS volunteers who have made studies such as this one
possible. We thank T. A. G. Rittenhouse, F. Beaudry, A. R. Rissman, and
4 anonymous reviewers for comments and D. Helmers for technical
assistance. We gratefully acknowledge funding from the National
Aeronautics and Space Administration (NASA) Biodiversity Program and the
NASA Interdisciplinary Sciences Program. T. P. A. acknowledges support
from National Science Foundation (Cooperative Agreement EPS-0814372).
NR 39
TC 15
Z9 15
U1 1
U2 64
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0888-8892
J9 CONSERV BIOL
JI Conserv. Biol.
PD OCT
PY 2012
VL 26
IS 5
BP 821
EP 829
DI 10.1111/j.1523-1739.2012.01867.x
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 001UB
UT WOS:000308484500008
PM 22731630
ER
PT J
AU Pollnac, RB
Kotowicz, D
AF Pollnac, Richard B.
Kotowicz, Dawn
TI Post Tsunami Job Satisfaction Among the Fishers of Na Pru Village, on
the Andaman Sea Coast of Thailand
SO SOCIAL INDICATORS RESEARCH
LA English
DT Article
DE Job satisfaction; Small-scale fishermen; Thailand
ID MANAGEMENT; POLICY
AB The paper examines job satisfaction among fishers in a tsunami-impacted area on the Andaman coast of Thailand. Following the tsunami, many predicted that fishers would be reluctant to resume their fishing activities. Observations in the fishing communities, however, indicated that as soon as fishers obtained replacements for equipment damaged by the tsunami, they began to fish again. Nevertheless, most fishers reported they would change fishing type, and that if they had the opportunity they would leave fishing altogether. Whether or not these attitudes can be attributed solely to the impacts of the tsunami is not clear at this point, but this supposition is provided some support from data collected from small scale fishers in two towns near Bangkok in the Gulf of Thailand which reflected more positive attitudes towards the occupation. While attitudes towards the occupation are more negative than those reported for many other fisheries, the scores for the job satisfaction categories indicated that the sample means for all job satisfaction categories except Self-Actualisation are above the midpoint on the scales. This, in turn, indicates general satisfaction with the occupation-perhaps the challenge and adventure of the job are perceived as being a little too much following on the heels of the Indian Ocean tsunami that devastated the area. Hence, although fishers say that they would leave the occupation for another, it is unlikely that they will unless the alternate occupation, at the very least, meets the satisfactions provided by fishing.
C1 [Pollnac, Richard B.] Univ Rhode Isl, Kingston, RI 02881 USA.
[Kotowicz, Dawn] Univ Hawaii, Joint Inst Marine & Atmospher Res, Natl Marine Fisheries Serv, Honolulu, HI 96822 USA.
RP Pollnac, RB (reprint author), Univ Rhode Isl, Kingston, RI 02881 USA.
EM pollnac3@gmail.com
NR 12
TC 0
Z9 0
U1 2
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0303-8300
J9 SOC INDIC RES
JI Soc. Indic. Res.
PD OCT
PY 2012
VL 109
IS 1
BP 67
EP 80
DI 10.1007/s11205-012-0056-2
PG 14
WC Social Sciences, Interdisciplinary; Sociology
SC Social Sciences - Other Topics; Sociology
GA 004EO
UT WOS:000308663300006
ER
PT J
AU Nguyen, TA
Do, M
Gerevini, AE
Serina, I
Srivastava, B
Kambhampati, S
AF Tuan Anh Nguyen
Minh Do
Gerevini, Alfonso Emilio
Serina, Ivan
Srivastava, Biplav
Kambhampati, Subbarao
TI Generating diverse plans to handle unknown and partially known user
preferences
SO ARTIFICIAL INTELLIGENCE
LA English
DT Article
DE Planning; Partial preferences; Diverse plans; Heuristics; Search
ID APPROXIMATE SOLUTION SETS; OPTIMIZATION PROBLEMS; PLANNING GRAPH; SEARCH
AB Current work in planning with preferences assumes that user preferences are completely specified, and aims to search for a single solution plan to satisfy these. In many real world planning scenarios, however, the user may provide no knowledge or at best partial knowledge of her preferences with respect to a desired plan. In such situations, rather than presenting a single plan as the solution, the planner must instead provide a set of plans containing one or more plans that are similar to the one that the user really prefers. In this paper, we first propose the usage of different measures to capture the quality of such plan sets. These are domain-independent distance measures based on plan elements (such as actions, states, or causal links) if no knowledge of the user preferences is given, or the Integrated Convex Preference (ICP) measure in case incomplete knowledge of such preferences is provided. We then investigate various heuristic approaches to generate sets of plans in accordance with these measures, and present empirical results that demonstrate the promise of our methods. (c) 2012 Elsevier B.V. All rights reserved.
C1 [Tuan Anh Nguyen; Kambhampati, Subbarao] Arizona State Univ, Sch Comp Informat & Decis Syst Engn, Tempe, AZ 85281 USA.
[Minh Do] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gerevini, Alfonso Emilio] Univ Brescia, Dipartimento Ingn Informaz, I-25123 Brescia, Italy.
[Serina, Ivan] Free Univ Bozen Bolzano, I-39042 Bressanone, Italy.
[Srivastava, Biplav] IBM India Res Lab, New Delhi, India.
[Srivastava, Biplav] IBM India Res Lab, Bangalore, Karnataka, India.
RP Nguyen, TA (reprint author), Arizona State Univ, Sch Comp Informat & Decis Syst Engn, Brickyard Suite 501,699 S Mill Ave, Tempe, AZ 85281 USA.
EM natuan@asu.edu; minh.b.do@nasa.gov; gerevini@ing.unibs.it;
ivan.serina@unibz.it; sbiplav@in.ibm.com; rao@asu.edu
OI SERINA, Ivan/0000-0002-7785-9492
FU IBM Faculty Award; NSF grant [IIS2013308139]; ONR [N00014-09-1-0017,
N00014-07-1-1049, N000140610058]; Lockheed Martin subcontract as part of
the DARPA Integrated Learning program [TT0687680]; Science Foundation of
Arizona fellowship
FX We thank Menkes van den Briel for drawing our attention to ICP measure
initially. Kambhampati's research is supported in part by an IBM Faculty
Award, the NSF grant IIS2013308139, ONR grants N00014-09-1-0017,
N00014-07-1-1049, N000140610058, and by a Lockheed Martin subcontract
TT0687680 to ASU as part of the DARPA Integrated Learning program. Tian
Nguyen was also supported by a Science Foundation of Arizona fellowship.
NR 56
TC 10
Z9 10
U1 0
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0004-3702
EI 1872-7921
J9 ARTIF INTELL
JI Artif. Intell.
PD OCT
PY 2012
VL 190
BP 1
EP 31
DI 10.1016/j.artint.2012.05.005
PG 31
WC Computer Science, Artificial Intelligence
SC Computer Science
GA 002FJ
UT WOS:000308517100001
ER
PT J
AU Griffin, W
Wang, Y
Berrios, D
Olano, M
AF Griffin, Wesley
Wang, Yu
Berrios, David
Olano, Marc
TI Real-Time GPU Surface Curvature Estimation on Deforming Meshes and
Volumetric Data Sets
SO IEEE TRANSACTIONS ON VISUALIZATION AND COMPUTER GRAPHICS
LA English
DT Article
DE Real-time rendering; GPU; geometry shader; curvature; line drawing;
ambient occlusion
ID SHAPE
AB Surface curvature is used in a number of areas in computer graphics, including texture synthesis and shape representation, mesh simplification, surface modeling, and nonphotorealistic line drawing. Most real-time applications must estimate curvature on a triangular mesh. This estimation has been limited to CPU algorithms, forcing object geometry to reside in main memory. However, as more computational work is done directly on the GPU, it is increasingly common for object geometry to exist only in GPU memory. Examples include vertex skinned animations and isosurfaces from GPU-based surface reconstruction algorithms. For static models, curvature can be precomputed and CPU algorithms are a reasonable choice. For deforming models where the geometry only resides on the GPU, transferring the deformed mesh back to the CPU limits performance. We introduce a GPU algorithm for estimating curvature in real time on arbitrary triangular meshes. We demonstrate our algorithm with curvature-based NPR feature lines and a curvature-based approximation for an ambient occlusion. We show curvature computation on volumetric data sets with a GPU isosurface extraction algorithm and vertex-skinned animations. We present a graphics pipeline and CUDA implementation. Our curvature estimation is up to similar to 18x faster than a multithreaded CPU benchmark.
C1 [Griffin, Wesley; Wang, Yu; Olano, Marc] Univ Maryland Baltimore Cty, Dept Comp Sci & Elect Engn, Baltimore, MD 21250 USA.
[Berrios, David] NASA, Goddard Space Flight Ctr, Sci Data Proc Branch, Greenbelt, MD 20771 USA.
RP Griffin, W (reprint author), Univ Maryland Baltimore Cty, Dept Comp Sci & Elect Engn, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM griffin5@cs.umbc.edu; zf89375@umbc.edu; david.h.berrios@nasa.gov;
olano@umbc.edu
FU Maryland Industrial Partnerships (MIPS)
FX Thanks to the many reviewers, whose comments have greatly improved this
paper. Szymon Rusinkiewicz for the trimesh2 library [37]. Christopher
Twigg for the Skinning Mesh Animations data [38]. Stefan Rottger for the
volume data sets [39]. Lee Perry-Smith for the head scan [40]. White et
al. for the toss and coin data sets [41]. Ingo Wald for the hand and
fairy data sets [42]. NVIDIA for providing the Quadro FX5800. Maryland
Industrial Partnerships (MIPS) for providing support.
NR 42
TC 4
Z9 6
U1 0
U2 8
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1077-2626
EI 1941-0506
J9 IEEE T VIS COMPUT GR
JI IEEE Trans. Vis. Comput. Graph.
PD OCT
PY 2012
VL 18
IS 10
BP 1603
EP 1613
DI 10.1109/TVCG.2012.113
PG 11
WC Computer Science, Software Engineering
SC Computer Science
GA 985VO
UT WOS:000307298800003
PM 22508906
ER
PT J
AU Landry, SJ
Farley, T
Hoang, T
Stein, B
AF Landry, Steven J.
Farley, Todd
Ty Hoang
Stein, Brian
TI A distributed scheduler for air traffic flow management
SO JOURNAL OF SCHEDULING
LA English
DT Article
DE Air traffic flow management; Distributed scheduler; Air traffic arrival
scheduling; Decision support
ID GROUND-HOLDING PROBLEM; AIRPORT
AB A system was developed to efficiently schedule aircraft into congested resources over long ranges and present that schedule as a decision support system. The scheduling system consists of a distributed network of independent schedulers, loosely coupled by sharing capacity information. This loose coupling insulates the schedules from uncertainty in long-distance estimations of arrival times, while allowing precise short-term schedules to be constructed. This "rate profile" mechanism allows feasible schedules to be produced over long ranges, essentially constructing precise short-range schedules that also ensure that future scheduling problems are solvable while meeting operational constraints. The system was tested operationally and demonstrated reduced airborne delay and improved coordination.
C1 [Landry, Steven J.; Farley, Todd; Ty Hoang] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stein, Brian] Methods Corp, English Creek, NJ USA.
RP Landry, SJ (reprint author), Purdue Univ, Sch Ind Engn, 315 N Grant St, W Lafayette, IN 47906 USA.
EM slandry@purdue.edu
NR 34
TC 2
Z9 2
U1 0
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1094-6136
J9 J SCHEDULING
JI J. Sched.
PD OCT
PY 2012
VL 15
IS 5
BP 537
EP 551
DI 10.1007/s10951-012-0271-3
PG 15
WC Engineering, Manufacturing; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA 998MD
UT WOS:000308242600002
ER
PT J
AU Mishchenko, MI
Liu, L
Geogdzhayev, IV
Li, J
Carlson, BE
Lacis, AA
Cairns, B
Travis, LD
AF Mishchenko, Michael I.
Liu, Li
Geogdzhayev, Igor V.
Li, Jing
Carlson, Barbara E.
Lacis, Andrew A.
Cairns, Brian
Travis, Larry D.
TI Aerosol retrievals from channel-1 and -2 AVHRR radiances: Long-term
trends updated and revisited
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Tropospheric aerosols; Remote sensing; Global climate change;
Brightening and dimming
ID UNIFIED SATELLITE CLIMATOLOGY; HIGH-RESOLUTION RADIOMETER; RADIATIVE
PROPERTIES; INFORMATION-CONTENT; SOLAR IRRADIANCE; EARTHS SURFACE; BLACK
CARBON; ABSORPTION; ATMOSPHERE; SCATTERING
AB The nominal Global. Aerosol Climatology Project (GACP) record of aerosol optical thickness (AOT) and Angstrom exponent (AE) over the oceans is extended by 6 months to cover the period from August 1981 through December 2005. The most recent 4-year segment reveals no significant short-term tendencies in globally and hemispherically averaged AOTs and AEs. This finding is consistent with contemporaneous MODIS and MISR results and the accumulating evidence of a gradual transition from global brightening to global dimming. We also analyze the retrieval implications of allowing the imaginary part of the aerosols refractive index Im(m) to change over the duration of the GACP record. Our sensitivity study shows that increasing Im(m) from 0.003 during the 4-year pre-Pinatubo period up to 0.007 during the most recent 4-year segment of GACP data eliminates the previously identified long-term decreasing AOT trend. Should this long-term trend in Im(m) be real then it would cause the global absorption AOT over the oceans to more than double and the global single-scattering albedo to decrease from similar to 0.95 to similar to 0.88. Such changes could make tropospheric aerosols significant contributors to the recent surface temperature increase. Published by Elsevier Ltd.
C1 [Mishchenko, Michael I.; Li, Jing; Carlson, Barbara E.; Lacis, Andrew A.; Cairns, Brian; Travis, Larry D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Liu, Li; Geogdzhayev, Igor V.] Columbia Univ, New York, NY 10025 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
RI Li, Jing/J-2397-2014; Mishchenko, Michael/D-4426-2012;
OI Li, Jing/0000-0002-0540-0412; Cairns, Brian/0000-0002-1980-1022
FU NASA
FX This research was supported by the NASA Glory Mission Project supervised
by Hal Mating and by the NASA Remote Sensing Theory Program managed by
Lucia Tsaoussi.
NR 84
TC 11
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U1 0
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD OCT
PY 2012
VL 113
IS 15
BP 1974
EP 1980
DI 10.1016/j.jqsrt.2012.05.006
PG 7
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 990EY
UT WOS:000307615000014
ER
PT J
AU Norris, KJ
Wong, VK
Onishi, T
Lohn, AJ
Coleman, E
Tompa, GS
Kobayashi, NP
AF Norris, Kate J.
Wong, Vernon K.
Onishi, Takehiro
Lohn, Andrew J.
Coleman, Elane
Tompa, Gary S.
Kobayashi, Nobuhiko P.
TI Reflection absorption infrared spectroscopy analysis of the evolution of
ErSb on InSb
SO SURFACE SCIENCE
LA English
DT Article
DE ErSb; InSb; Infrared absorption; MOCVD; AFM; Evolution; Island; Surface
coverage
AB We discuss an ex-situ monitoring technique based on glancing-angle infrared-absorption used to determine small amounts of erbium antimonide (ErSb) deposited on an indium antimonide (InSb) layer epitaxially grown on an InSb (100) substrate by low pressure metal organic chemical vapor deposition (MOCVD). Infrared absorption from the indium-hydrogen (In - H) stretching mode at 1754.5 cm(-1) associated with a top most surface of an epitaxial InSb layer was used to compare varying levels of surface coverage with ErSb. Among four samples of varying coverage of ErSb deposition (7.2 to 21.5 monolayers), detected infrared absorption peaks distinct to In - H weakened as ErSb surface coverage increased. In the early stage of ErSb deposition, our study suggests that outermost indium atoms in the InSb buffer layer are replaced by Er resulting in increase in absorption associated with the In - H mode. Using this simple ex-situ technique, we show that it is possible to calibrate the amount of ErSb deposited atop each individual InSb substrate for depositions of few to tens of monolayers. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Norris, Kate J.; Wong, Vernon K.; Onishi, Takehiro; Lohn, Andrew J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
[Norris, Kate J.; Wong, Vernon K.; Lohn, Andrew J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Adv Studies Labs, Nanostruct Energy Convers Technol & Res NECTAR, Moffett Field, CA USA.
[Norris, Kate J.; Wong, Vernon K.; Lohn, Andrew J.; Kobayashi, Nobuhiko P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Coleman, Elane; Tompa, Gary S.] Struct Mat Ind Inc, Piscataway, NJ USA.
RP Kobayashi, NP (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
EM nobby@soe.ucsc.edu
RI Kobayashi, Nobuhiko/E-3834-2012
FU DARPA/DSO; ONR; DoE
FX This work is funded by the DARPA/DSO, ONR, and DoE. We are grateful to
Hewlett-Packard Laboratories for their continuous support in our work.
We thank the Materials Analysis for Collaborative Science (Univ. of
California Santa Cruz and NASA Ames Research Center) for their
facilities and assistance in our studies.
NR 12
TC 1
Z9 1
U1 0
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0039-6028
J9 SURF SCI
JI Surf. Sci.
PD OCT
PY 2012
VL 606
IS 19-20
BP 1556
EP 1559
DI 10.1016/j.susc.2012.06.004
PG 4
WC Chemistry, Physical; Physics, Condensed Matter
SC Chemistry; Physics
GA 991JN
UT WOS:000307697400015
ER
PT J
AU Okutsu, M
Yam, CH
Longuski, JM
Strange, NJ
AF Okutsu, Masataka
Yam, Chit Hong
Longuski, James M.
Strange, Nathan J.
TI Cassini Saturn-escape trajectories to Jupiter, Uranus, and Neptune
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Cassini; Satellite-aided escape; Satellite tour; Tour design
ID MISSION; SYSTEM
AB Potential encore-mission scenarios have been considered for the Cassini mission. In this paper we discuss one of the end-of-life scenarios in which the Cassini spacecraft could perform a Saturn escape via gravity assists from Titan. It is shown that such satellite-aided escape requires a small deterministic maneuver (e.g., Delta nu <50 m/s), but provides enough energy for the Cassini spacecraft to reach a range of targets in our Solar System, as close to the Sun as the asteroid belt or as far as the Kuiper belt. The escape sequence could be initiated from an arbitrary point during the on-going Cassini mission. Example tours are presented in which the final Titan flyby places the spacecraft into ballistic trajectories that reach Jupiter, Uranus, and Neptune. After years of heliocentric flight, the spacecraft could impact on the target gas giant or perform a flyby to escape from the Solar System (if not to another destination). The concept can be generalized to a new kind of missions, including nested-grand tours, which may involve satellite-aided captures and escapes at more than one planet. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Okutsu, Masataka; Yam, Chit Hong; Longuski, James M.] Purdue Univ, W Lafayette, IN 47907 USA.
[Strange, Nathan J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Okutsu, M (reprint author), Purdue Univ, Armstrong Hall,701 W Stadium Ave, W Lafayette, IN 47907 USA.
EM okutsu@gmail.com
FU Jet Propulsion Laboratory (JPL), California Institute of Technology;
National Aeronautics and Space Administration; JPL [1283234]
FX This research was funded by the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. A portion of work at Purdue
University has been supported under JPL Contract 1283234 (with Jeremy B.
Jones as the Technical Manager). We are indebted to Robert T. Mitchell
and Jeremy B. Jones for their support and guidance.
NR 30
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U1 1
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2012
VL 79
BP 157
EP 167
DI 10.1016/j.actaastro.2012.04.034
PG 11
WC Engineering, Aerospace
SC Engineering
GA 971MQ
UT WOS:000306208400017
ER
PT J
AU Cohen, BA
Chavers, DG
Ballard, BW
AF Cohen, Barbara A.
Chavers, D. Gregory
Ballard, Benjamin W.
TI NASA'S Robotic Lunar Lander Development Project
SO ACTA ASTRONAUTICA
LA English
DT Review
DE Spacecraft; Lander; Moon; Systems engineering; Airless bodies; Lunar
science
AB Over the last 5 years, NASA has invested in development and risk-reduction activities for a new generation of planetary landers capable of carrying instruments and technology demonstrations to the lunar surface and other airless bodies. The Robotic Lunar Lander Development Project (RLLDP) is jointly implemented by NASA Marshall Space Flight Center (MSFC) and the Johns Hopkins University Applied Physics Laboratory (APL). The RLLDP team has produced mission architecture designs for multiple airless body missions to meet both science and human precursor mission needs. The mission architecture concept studies encompass small, medium, and large landers, with payloads from a few tens of kilograms to over 1000 kg, to the Moon and other airless bodies. To mature these concepts, the project has made significant investments in technology risk reduction in focused subsystems. In addition, many lander technologies and algorithms have been tested and demonstrated in an integrated systems environment using free-Hying test articles. These design and testing investments have significantly reduced development risk for airless body landers, thereby reducing overall risk and associated costs for future missions. Published by Elsevier Ltd.
C1 [Cohen, Barbara A.; Chavers, D. Gregory] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Ballard, Benjamin W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Cohen, BA (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM Barbara.A.Cohen@nasa.gov
FU Robotic Lunar Exploration Program; Lunar Precursor Robotics Program;
International Lunar Network Project; Exploration Precursor Robotic
Program; Planetary Science Decadal Survey; Robotic Lunar Lander
Development Project at NASA Headquarters
FX This work was supported by the Robotic Lunar Exploration Program, the
Lunar Precursor Robotics Program, the International Lunar Network
Project, the Exploration Precursor Robotic Program, the Planetary
Science Decadal Survey, and the Robotic Lunar Lander Development Project
at NASA Headquarters, supplemented by internal research and development
efforts at the Applied Physics Laboratory and Marshall Space Flight
Center. Many RLLDP team members contributed to the research in this
paper including: at MSFC, Julie A. Bassler, Jeffrey T. Farmer, Todd M.
Freestone, Daniel L. Gunter, Monica S. Hammond, Michael R. Hannan,
Lawrence D. Hill, Danny W. Harris, Todd A. Holloway, John E. Lowery,
Brian D. Mu lac, and Cynthia D. Stemple; and at APL, David Artis, Teresa
Betenbaugh, Timothy J. Cole, Doug S. Eng, Sanae Kubota, Paul Lafferty,
Timothy G. McGee, Brian J. Morse, Deva Ponnusamy, and Cheryl L B. Reed.
This research has made use of NASA's Astrophysics Data System (ADS).
NR 34
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U1 1
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2012
VL 79
BP 221
EP 240
DI 10.1016/j.actaastro.2012.03.025
PG 20
WC Engineering, Aerospace
SC Engineering
GA 971MQ
UT WOS:000306208400023
ER
PT J
AU Scandaliato, AL
Liou, MS
AF Scandaliato, Angelo L.
Liou, Meng-Sing
TI AUSM-Based High-Order Solution for Euler Equations
SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS
LA English
DT Article
DE Shock capturing; advection upwind splitting; Euler equations; weighted
essentially non-oscillatory; monotonicity preserving
ID ESSENTIALLY NONOSCILLATORY SCHEMES; HYPERBOLIC CONSERVATION-LAWS;
EFFICIENT IMPLEMENTATION; WENO SCHEMES; SEQUEL
AB In this paper we demonstrate the accuracy and robustness of combining the advection upwind splitting method (AUSM), specifically AUSM(+)-UP 191, with high-order upwind-biased interpolation procedures, the weighted essentially non-oscillatory (WENO-JS) scheme 181 and its variations 12,71, and the monotonicity preserving (MP) scheme 1161, for solving the Euler equations. MP is found to be more effective than the three WEN variations studied. AUSM(+)-UP is also shown to be free of the so-called "carbuncle" phenomenon with the high-order interpolation. The characteristic variables are preferred for interpolation after comparing the results using primitive and conservative variables, even though they require additional matrix-vector operations. Results using the Roe flux with an entropy fix and the Lax-Friedrichs approximate Riemann solvers are also included for comparison. In addition, four reflective boundary condition implementations are compared for their effects on residual convergence and solution accuracy. Finally, a measure for quantifying the efficiency of obtaining high order solutions is proposed; the measure reveals that a maximum return is reached after which no improvement in accuracy is possible for a given grid size.
C1 [Scandaliato, Angelo L.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Liou, Meng-Sing] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Liou, MS (reprint author), Ohio Aerosp Inst, Cleveland, OH 44142 USA.
EM ascandal@ucsd.edu; meng-sing.liou@nasa.gov
FU NASA, Aeronautics Mission Directorate
FX This work has been supported by the Subsonic Fixed Wing and Supersonics
Projects under the NASA's Fundamental Aeronautics Program, Aeronautics
Mission Directorate. We also thank H.T. Huynh of NASA Glenn Research
Center for his help with the MP method.
NR 19
TC 3
Z9 3
U1 0
U2 13
PU GLOBAL SCIENCE PRESS
PI WANCHAI
PA ROOM 3208, CENTRAL PLAZA, 18 HARBOUR RD, WANCHAI, HONG KONG 00000,
PEOPLES R CHINA
SN 1815-2406
J9 COMMUN COMPUT PHYS
JI Commun. Comput. Phys.
PD OCT
PY 2012
VL 12
IS 4
BP 1096
EP 1120
DI 10.4208/cicp.250311.081211a
PG 25
WC Physics, Mathematical
SC Physics
GA 938ZX
UT WOS:000303773900008
ER
PT J
AU Chen, MW
Lemon, CL
Guild, TB
Schulz, M
Roeder, JL
Le, G
AF Chen, Margaret W.
Lemon, Colby L.
Guild, Timothy B.
Schulz, Michael
Roeder, James L.
Le, Guan
TI Comparison of self-consistent simulations with observed magnetic field
and ion plasma parameters in the ring current during the 10 August 2000
magnetic storm
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID DAWN-DUSK ASYMMETRY; INNER MAGNETOSPHERE; GEOMAGNETIC STORMS;
GEOSYNCHRONOUS ORBIT; SOLAR-WIND; MODEL; SHEET; PHASE; ELECTRODYNAMICS;
SPECIFICATION
AB We assess whether magnetically and electrically self-consistent ring current simulations can account simultaneously for in situ magnetic field and ion flux measurements in the inner magnetosphere during the large 10 August 2000 storm (min Dst = -107 nT). We use the Rice Convection Model-Equilibrium (RCM-E) and drive it with time-dependent magnetic field, electric field, and plasma boundary conditions that are guided by empirical and assimilative models. Comparisons of the simulated and observed magnetic field from Geostationary Operational Environmental Satellites (GOES) and observed proton differential flux spectra from Los Alamos National Laboratory (LANL) satellites are made at geosynchronous orbit (GEO). Similarly, simulated and observed magnetic field and proton density and temperature are compared along the orbit of Polar (r similar to 1.8-9 R-E) for the event. The simulated and observed magnetic field components agree reasonably well at GEO and along the orbit of Polar. However, since the effects of substorm dipolarizations are not explicitly modeled, the simulation fails to reproduce observed sawtooth fluctuations in the magnetic field. Over energies from 1 to 150 keV, the RCM-E reproduced well the ion dispersion features in the LANL 1994-084 ion differential flux spectra over energies at GEO and proton densities and temperatures calculated from Polar proton flux measurements. Thus, the RCM-E simulations can account simultaneously for in situ magnetic field and ion flux measurements for the 10 August 2000 storm. This demonstrates that a self-consistent model can produce realistic features of the storm time inner magnetosphere.
C1 [Chen, Margaret W.; Lemon, Colby L.; Guild, Timothy B.; Roeder, James L.] Aerosp Corp, Space Sci Applicat Lab, El Segundo, CA 90009 USA.
[Schulz, Michael] Lockheed Martin Adv Technol Ctr, Palo Alto, CA USA.
[Le, Guan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chen, MW (reprint author), Aerosp Corp, Space Sci Applicat Lab, MS M2-260,POB 92957, El Segundo, CA 90009 USA.
EM margaret.w.chen@aero.org
RI Le, Guan/C-9524-2012; Chen, Margaret/C-9658-2013
OI Le, Guan/0000-0002-9504-5214; Chen, Margaret/0000-0001-7771-4771
FU NASA HGIP [NNX10AQ41G]; NSF GEM [ATM-0902832, AGS-1003874]
FX We thank our collaborators at Rice for the use of their portions of the
RCM-E code and for ongoing discussions of numerical and physical aspects
of RCM-E development. We used the IRBEM (formerly ONERA) library of
magnetic field models, geophysical coordinate transformations, and field
line tracing routines. The OMNI data were obtained from the GSFC/SPDF
OMNIWeb interface at http://omniweb.gsfc.nasa.gov. We thank numerous
geomagnetic observatories (Kakioka (JMA), Honolulu and San Juan (USGS),
Hermanus (RSA), Alibag (IIG)), NiCT, INTERMAGNET, and many others) for
their cooperation in making the SYM-H index available. The authors thank
C. T. Russell for the use of the data from the Magnetic Field
Investigation and T. A. Fritz for the use of the data from the Charge
and Mass Magnetospheric Ion Composition Experiment on the NASA Polar
satellite. We are grateful for helpful discussions with our colleagues
J. F. Fennell and T. P. O'Brien at The Aerospace Corporation. The
research at The Aerospace Corporation was supported in part by NASA HGIP
grant NNX10AQ41G, NSF GEM grant ATM-0902832, and NSF GEM grant
AGS-1003874.
NR 55
TC 4
Z9 4
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 29
PY 2012
VL 117
AR A09232
DI 10.1029/2012JA017788
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 131EB
UT WOS:000317974100003
ER
PT J
AU Buczkowski, DL
Wyrick, DY
Iyer, KA
Kahn, EG
Scully, JEC
Nathues, A
Gaskell, RW
Roatsch, T
Preusker, F
Schenk, PM
Le Corre, L
Reddy, V
Yingst, RA
Mest, S
Williams, DA
Garry, WB
Barnouin, OS
Jaumann, R
Raymond, CA
Russell, CT
AF Buczkowski, D. L.
Wyrick, D. Y.
Iyer, K. A.
Kahn, E. G.
Scully, J. E. C.
Nathues, A.
Gaskell, R. W.
Roatsch, T.
Preusker, F.
Schenk, P. M.
Le Corre, L.
Reddy, V.
Yingst, R. A.
Mest, S.
Williams, D. A.
Garry, W. B.
Barnouin, O. S.
Jaumann, R.
Raymond, C. A.
Russell, C. T.
TI Large-scale troughs on Vesta: A signature of planetary tectonics
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID 21 LUTETIA; 433 EROS; DAWN; HETEROGENEITY; DISPLACEMENT; GROWTH; SYSTEM;
FAULTS
AB Images of Vesta taken by the Dawn spacecraft reveal large-scale linear structural features on the surface of the asteroid. We evaluate the morphology of the Vesta structures to determine what processes caused them to form and what implications this has for the history of Vesta as a planetary body. The dimensions and shape of these features suggest that they are graben similar to those observed on terrestrial planets, not fractures or grooves such as are found on smaller asteroids. As graben, their vertical displacement versus length relationship could be evaluated to describe and interpret the evolution of the component faults. Linear structures are commonly observed on smaller asteroids and their formation has been tied to impact events. While the orientation of the large-scale Vesta structures does imply that their formation is related to the impact events that formed the Rheasilvia and Veneneia basins, their size and morphology is greatly different from impact-formed fractures on the smaller bodies. This is consistent with new analyses that suggest that Vesta is fully differentiated, with a mantle and core. We suggest that impact into a differentiated asteroid such as Vesta could result in graben, while grooves and fractures would form on undifferentiated asteroids. Citation: Buczkowski, D. L., et al. (2012), Large-scale troughs on Vesta: A signature of planetary tectonics, Geophys. Res. Lett., 39, L18205, doi: 10.1029/2012GL052959.
C1 [Buczkowski, D. L.; Iyer, K. A.; Kahn, E. G.; Barnouin, O. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Wyrick, D. Y.] SW Res Inst, San Antonio, TX USA.
[Scully, J. E. C.; Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Nathues, A.; Le Corre, L.; Reddy, V.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
[Gaskell, R. W.; Yingst, R. A.; Mest, S.; Garry, W. B.] Planetary Sci Inst, Tucson, AZ USA.
[Roatsch, T.; Preusker, F.; Jaumann, R.] DLR, Inst Planetary Res, Berlin, Germany.
[Schenk, P. M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Reddy, V.] Univ N Dakota, Dept Earth Syst Sci & Policy, Grand Forks, ND 58201 USA.
[Williams, D. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Buczkowski, DL (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM debra.buczkowski@jhuapl.edu
RI Russell, Christopher/E-7745-2012; Garry, Brent/I-5920-2013; Barnouin,
Olivier/I-7475-2015; Buczkowski, Debra/I-7842-2015; Iyer,
Kaushik/H-1411-2016;
OI Russell, Christopher/0000-0003-1639-8298; Barnouin,
Olivier/0000-0002-3578-7750; Buczkowski, Debra/0000-0002-4729-7804;
Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932
FU Dawn Science, Operations and other Instrument Teams; National
Aeronautics and Space Administration [NNX10AR58G]
FX The authors gratefully acknowledge the Framing Camera team, as well as
the support of the Dawn Science, Operations and other Instrument Teams.
This research is supported by the National Aeronautics and Space
Administration under grant NNX10AR58G issued through the Science Mission
Directorate Dawn at Vesta Participating Science Program.
NR 27
TC 28
Z9 28
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 29
PY 2012
VL 39
AR L18205
DI 10.1029/2012GL052959
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 014ZY
UT WOS:000309415700002
ER
PT J
AU Yatheendradas, S
Lidard, CDP
Koren, V
Cosgrove, BA
De Goncalves, LGG
Smith, M
Geiger, J
Cui, ZT
Borak, J
Kumar, SV
Toll, DL
Riggs, G
Mizukami, N
AF Yatheendradas, Soni
Lidard, Christa D. Peters
Koren, Victor
Cosgrove, Brian A.
De Goncalves, Luis G. G.
Smith, Michael
Geiger, Jim
Cui, Zhengtao
Borak, Jordan
Kumar, Sujay V.
Toll, David L.
Riggs, George
Mizukami, Naoki
TI Distributed assimilation of satellite-based snow extent for improving
simulated streamflow in mountainous, dense forests: An example over the
DMIP2 western basins
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID REMOTE-SENSING DATA; LAND-SURFACE MODEL; COVERED AREA; WATER EQUIVALENT;
HYDROLOGIC MODEL; SIERRA-NEVADA; RIVER-BASIN; MODIS; VARIABILITY;
VEGETATION
AB Snow cover area affects snowmelt, soil moisture, evapotranspiration, and ultimately streamflow. For the Distributed Model Intercomparison Project - Phase 2 Western basins, we assimilate satellite-based fractional snow cover area (fSCA) from the Moderate Resolution Imaging Spectroradiometer, or MODIS, into the National Weather Service (NWS) SNOW-17 model. This model is coupled with the NWS Sacramento Heat Transfer (SAC-HT) model inside the National Aeronautics and Space Administration's (NASA) Land Information System. SNOW-17 computes fSCA from snow water equivalent (SWE) values using an areal depletion curve. Using a direct insertion, we assimilate fSCAs in two fully distributed ways: (1) we update the curve by attempting SWE preservation, and (2) we reconstruct SWEs using the curve. The preceding are refinements of an existing simple, conceptually guided NWS algorithm. Satellite fSCA over dense forests inadequately accounts for below-canopy snow, degrading simulated streamflow upon assimilation during snowmelt. Accordingly, we implement a below-canopy allowance during assimilation. This simplistic allowance and direct insertion are found to be inadequate for improving calibrated results, still degrading them as mentioned above. However, for streamflow volume for the uncalibrated runs, we obtain: (1) substantial to major improvements (64-81%) as a percentage of the control run residuals (or distance from observations), and (2) minor improvements (16-22%) as a percentage of observed values. We highlight the need for detailed representations of canopy-snow optical radiative transfer processes in mountainous, dense forest regions if assimilation-based improvements are to be seen in calibrated runs over these areas.
C1 [Yatheendradas, Soni; Lidard, Christa D. Peters; Borak, Jordan; Kumar, Sujay V.; Toll, David L.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Yatheendradas, Soni; Borak, Jordan] Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA.
[Koren, Victor; Cosgrove, Brian A.; Smith, Michael; Cui, Zhengtao; Mizukami, Naoki] NOAA, Natl Weather Serv, Off Hydrol Dev, Hydrol Lab, Silver Spring, MD 20910 USA.
[De Goncalves, Luis G. G.] DMD CPTEC INPE, Grp Data Assimilat Dev, Cachoeira Paulista, Brazil.
[Kumar, Sujay V.] Sci Applicat Int Corp, Beltsville, MD USA.
[Riggs, George] Sci Syst & Applicat Inc, Lanham, MD USA.
[Riggs, George] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
[Mizukami, Naoki] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Yatheendradas, S (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
EM soni.yatheendradas@nasa.gov
RI de Goncalves, Luis Gustavo/G-2522-2012; Kumar, Sujay/B-8142-2015;
OI de Goncalves, Luis Gustavo/0000-0002-1571-0916
FU NASA Applied Sciences Program Decisions-CAN [NN-H-04-Z-YO-010-C]
FX We gratefully acknowledge the support from the NASA Applied Sciences
Program Decisions-CAN proposal NN-H-04-Z-YO-010-C (PI: Restrepo). We
also acknowledge helpful science and project scheduling discussions with
Scott Rheingrover, provision of the correct aesc19_rms code by Eric
Anderson (NOAA, retired), data and basin comparison correspondence with
Robert Rice (UC Merced), MODIS data and assimilation communications with
Kristi Arsenault (GMU/CREW) and Dorothy Hall and James Foster
(NASA/GSFC), and in situ snow data initially provided by NOHRSC and the
DMIP2 project. We greatly appreciate the useful review comments and
suggestions provided by Editor John Selker, Associate Editor Martyn
Clark, two anonymous reviewers and Kristie Franz.
NR 95
TC 10
Z9 10
U1 2
U2 22
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 SEP 29
PY 2012
VL 48
AR W09557
DI 10.1029/2011WR011347
PG 18
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 015BR
UT WOS:000309420500001
ER
PT J
AU Borstad, CP
Khazendar, A
Larour, E
Morlighem, M
Rignot, E
Schodlok, MP
Seroussi, H
AF Borstad, C. P.
Khazendar, A.
Larour, E.
Morlighem, M.
Rignot, E.
Schodlok, M. P.
Seroussi, H.
TI A damage mechanics assessment of the Larsen B ice shelf prior to
collapse: Toward a physically-based calving law
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ANTARCTICA; TEMPERATURE; SYSTEM; MODEL
AB Calving is a primary process of mass ablation for glaciers and ice sheets, though it still eludes a general physical law. Here, we propose a calving framework based on continuum damage mechanics coupled with the equations of viscous deformation of glacier ice. We introduce a scalar damage variable that quantifies the loss of load-bearing surface area due to fractures and that feeds back with ice viscosity to represent fracture-induced softening. The calving law is a standard failure criterion for viscous damaging materials and represents a macroscopic brittle instability quantified by a critical or threshold damage. We constrain this threshold using the Ice Sheet System Model (ISSM) by inverting for damage on the Larsen B ice shelf prior to its 2002 collapse. By analyzing the damage distribution in areas that subsequently calved, we conclude that calving occurs after fractures have reduced the load-bearing capacity of the ice by 60 +/- 10%. Citation: Borstad, C. P., A. Khazendar, E. Larour, M. Morlighem, E. Rignot, M. P. Schodlok, and H. Seroussi (2012), A damage mechanics assessment of the Larsen B ice shelf prior to collapse: Toward a physically-based calving law, Geophys. Res. Lett., 39, L18502, doi: 10.1029/2012GL053317.
C1 [Borstad, C. P.; Khazendar, A.; Larour, E.; Rignot, E.; Schodlok, M. P.; Seroussi, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morlighem, M.; Rignot, E.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Schodlok, M. P.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Borstad, CP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 79-24, Pasadena, CA 91109 USA.
EM christopher.p.borstad@jpl.nasa.gov
RI Rignot, Eric/A-4560-2014; Morlighem, Mathieu/O-9942-2014
OI Rignot, Eric/0000-0002-3366-0481; Morlighem, Mathieu/0000-0001-5219-1310
FU Oak Ridge Associated Universities through a contract with NASA; JPL RTD
(Research, Technology and Development) program; NASA Cryospheric Science
program; MAP (Modeling, Analysis and Prediction) program; IDS
(Interdisciplinary Science) program
FX CB and HS were supported by appointments to the NASA Postdoctoral
Program at the Jet Propulsion Laboratory, administered by Oak Ridge
Associated Universities through a contract with NASA. Additional funding
provided by the JPL RTD (Research, Technology and Development) program
and NASA Cryospheric Science (AK and MS), MAP (Modeling, Analysis and
Prediction) and IDS (Interdisciplinary Science) programs.
NR 25
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U1 2
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2012
VL 39
AR L18502
DI 10.1029/2012GL053317
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 014ZS
UT WOS:000309415100007
ER
PT J
AU West, RA
Ajello, JM
Stevens, MH
Strobel, DF
Gladstone, GR
Evans, JS
Bradley, ET
AF West, R. A.
Ajello, J. M.
Stevens, M. H.
Strobel, D. F.
Gladstone, G. R.
Evans, J. S.
Bradley, E. T.
TI Titan airglow during eclipse
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB Solar XUV photons can provide enough energy to account for the observed nitrogen UV dayglow emissions above 800 km, but a small or sporadic contribution from energetic particles cannot be ruled out. Furthermore, ion production at altitudes deeper than 800 km as inferred from radio occultation cannot be produced by solar XUV stimulation and implies energy deposition from protons and oxygen ions. Here we examine UV spectra and visible-wavelength images of Titan in Saturn's shadow, when XUV stimulation is absent. UV emissions are observed in one of the three sets of spectra, and the intensity of these emissions is about a factor of 10 less than the peak intensity reported on the dayside. We observe visible-wavelength emissions for the first time. No horizontally resolved auroral structures are seen in the visible images. At visible wavelengths Titan has a global emission at the haze-top level that is not understood, although cosmic ray ionization and chemiluminescence are candidates needing further investigation. Citation: West, R. A., J. M. Ajello, M. H. Stevens, D. F. Strobel, G. R. Gladstone, J. S. Evans, and E. T. Bradley (2012), Titan airglow during eclipse, Geophys. Res. Lett., 39, L18204, doi: 10.1029/2012GL053230.
C1 [West, R. A.; Ajello, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stevens, M. H.] USN, Res Lab, Space Sci Div, Washington, DC 20375 USA.
[Strobel, D. F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Gladstone, G. R.] SW Res Inst, San Antonio, TX USA.
[Evans, J. S.] Computat Phys Inc, Springfield, VA USA.
[Bradley, E. T.] Univ Cent Florida, Dept Phys, Orlando, FL USA.
RP West, RA (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.a.west@jpl.nasa.gov
OI Stevens, Michael/0000-0003-1082-8955
FU Cassini-Huygens Mission through JPL [109303]; NASA Cassini Data Analysis
Program; Planetary Atmospheres Program; Cassini-Huygens mission; NASA
Astrobiology Institute; Jet Propulsion Laboratory, California Institute
of Technology; National Aeronautics and Space Administration
FX We thank Pascal Hedelt who supplied tables of H and CH4
densities in Titan's atmosphere. DFS was supported by the
Cassini-Huygens Mission through JPL contract 109303. JMA and MHS were
supported by the NASA Cassini Data Analysis Program and Planetary
Atmospheres Program. RAW was supported by the Cassini-Huygens mission
and by the NASA Astrobiology Institute. Part of this work was performed
by the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 19
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Z9 9
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2012
VL 39
AR L18204
DI 10.1029/2012GL053230
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 014ZS
UT WOS:000309415100006
ER
PT J
AU Wu, H
Kimball, JS
Li, HY
Huang, MY
Leung, LR
Adler, RF
AF Wu, Huan
Kimball, John S.
Li, Hongyi
Huang, Maoyi
Leung, L. Ruby
Adler, Robert F.
TI A new global river network database for macroscale hydrologic modeling
SO WATER RESOURCES RESEARCH
LA English
DT Article
AB Coarse-resolution (upscaled) river networks are critical inputs for runoff routing in macroscale hydrologic models. Recently, Wu et al. (2011) developed a hierarchical dominant river tracing (DRT) algorithm for automated extraction and spatial upscaling of river networks using fine-scale hydrography inputs. We applied the DRT algorithms using combined HydroSHEDS and HYDRO1k global fine-scale hydrography inputs and produced a new series of upscaled global river network data at multiple (1/16 degrees to 2 degrees) spatial resolutions. The new upscaled results are internally consistent and congruent with the baseline fine-scale inputs and should facilitate improved regional to global scale hydrologic simulations.
C1 [Wu, Huan; Adler, Robert F.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Wu, Huan; Adler, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Div Biol Sci, Polson, MT 59860 USA.
[Kimball, John S.] Univ Montana, Coll Forestry & Conservat, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
[Li, Hongyi; Huang, Maoyi; Leung, L. Ruby] Pacific NW Natl Lab, Richland, WA 99352 USA.
RP Wu, H (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM huanwu@umd.edu
RI Li, Hong-Yi/C-9143-2014; Wu, Huan/K-1003-2013; Huang, Maoyi/I-8599-2012
OI Li, Hong-Yi/0000-0001-5690-3610; Wu, Huan/0000-0003-2920-8860; Huang,
Maoyi/0000-0001-9154-9485
FU Gordon and Betty Moore Foundation; NASA Applied Sciences Program;
integrated earth system modeling (iESM) project; DOE Earth System
Modeling Program; U.S. DOE by Battelle Memorial Institute
[DE-AC06-76RLO1830]
FX This work was conducted at the University of Montana (UMT) and Earth
System Science Interdisciplinary Center (ESSIC), University of Maryland,
with financial support from the Gordon and Betty Moore Foundation, the
NASA Applied Sciences Program (Michael Goodman), and the integrated
earth system modeling (iESM) project funded by the DOE Earth System
Modeling Program. PNNL is operated for the U.S. DOE by Battelle Memorial
Institute under contract DE-AC06-76RLO1830. The authors would like to
thank John Lucotch (UMT) for assistance in data processing.
NR 5
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U1 0
U2 18
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 SEP 28
PY 2012
VL 48
AR W09701
DI 10.1029/2012WR012313
PG 5
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 015BN
UT WOS:000309420100001
ER
PT J
AU Fortenberry, RC
Huang, XC
Francisco, JS
Crawford, TD
Lee, TJ
AF Fortenberry, Ryan C.
Huang, Xinchuan
Francisco, Joseph S.
Crawford, T. Daniel
Lee, Timothy J.
TI Fundamental Vibrational Frequencies and Spectroscopic Constants of
HOCS+, HSCO+, and Isotopologues via Quartic Force Fields
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID CORRELATED MOLECULAR CALCULATIONS; PROTONATED CARBONYL SULFIDE;
GAUSSIAN-BASIS SETS; LASER SPECTROSCOPY; ABSORPTION-SPECTROSCOPY;
ANALYTIC EVALUATION; ROTATIONAL SPECTRA; ENERGY GRADIENTS;
WAVE-FUNCTIONS; TRANS-HOCO
AB Besides the nu(1) O-H stretching mode at 3435 cm(-1) for HOCS+, the fundamental vibrational frequencies for this cation and its HSCO+ isomer have not been determined experimentally. Because these systems are analogues to HOCO+, a detected interstellar molecule, and are believed to play an important role in reactions of OCS, which has also been detected in the interstellar medium, these cations are of importance to interstellar chemistry and reaction surface studies. This work provides the fundamental vibrational frequencies and spectroscopic constants computed with vibrational perturbation theory (VPT) at second order and the vibrational configuration interaction (VCI) method conjoined with the most accurate quartic force field (QFF) applied to date for these systems. Our computations match experiment to better than 2 cm(-1) for the known O-H stretch. Additionally, there is strong agreement in the prediction of the fundamentals across methods and choices of QFFs. The consistency in the computations and the correspondence for the known mode should give accurate reference data for the rovibrational spectra of these cations and their singly substituted isotopologues for D, O-18, and S-34.
C1 [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huang, Xinchuan] SETI, Mountain View, CA 94043 USA.
[Francisco, Joseph S.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Fortenberry, Ryan C.; Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA.
RP Fortenberry, RC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Ryan.C.Fortenberry@nasa.gov; Timothy.J.Lee@nasa.gov
RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012; Crawford,
Thomas/A-9271-2017
OI Crawford, Thomas/0000-0002-7961-7016
FU U.S. National Science Foundation [CHE-0741927, CHE-1058420]; NASA
[10-APRA10-0096, 10-APRA10-0167]; NASA/SETI Institute [NNX09AI49A,
NNX12AG96A]
FX Part of this work was funded by the U.S. National Science Foundation to
support the work by R.C.F. and T.D.C. through a Multi-User Chemistry
Research Instrumentation and Facility (CRIF:MU) award CHE-0741927 and
through award CHE-1058420. R.C.F. was also funded, in part, through the
NASA Postdoctoral Program administered by Oak Ridge Associated
Universities through a contract with NASA. The work undertaken by T.J.L.
was made possible through NASA Grant 10-APRA10-0096 and NASA Grant
10-APRA10-0167. X.H. also acknowledges funding from the NASA/SETI
Institute Cooperative Agreements NNX09AI49A and NNX12AG96A. We also
thank the reviewers for their insights which strengthened this paper,
especially with regards to Deff. The CheMVP program (courtesy
of Dr. Andrew Simmonett of the University of Georgia) was utilized in
the creation of the figures.
NR 52
TC 33
Z9 33
U1 0
U2 6
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD SEP 27
PY 2012
VL 116
IS 38
BP 9582
EP 9590
DI 10.1021/jp3073206
PG 9
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 011FG
UT WOS:000309149700016
PM 22950849
ER
PT J
AU Hughes, EJ
Sparling, LC
Carn, SA
Krueger, AJ
AF Hughes, E. J.
Sparling, L. C.
Carn, S. A.
Krueger, A. J.
TI Using horizontal transport characteristics to infer an emission height
time series of volcanic SO2
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID STRATOSPHERE; ERUPTIONS; CLOUDS
AB Characterizing the emission height of sulfur dioxide (SO2) from volcanic eruptions yields information about the strength of volcanic activity, and is crucial for the assessment of possible climate impacts and validation of satellite retrievals of SO2. Sensors such as the Ozone Monitoring Instrument (OMI) on the polar-orbiting Aura satellite provide accurate maps of the spatial distribution of volcanic SO2, but provide limited information on its vertical distribution. The goal of this work is to explore the possible use of a trajectory model in reconstructing both the temporal activity and injection altitude of volcanic SO2 from OMI column measurements observed far from the volcano. Using observations from the November 2006 eruption of Nyamuragira, back trajectories are run and statistical analyses are computed based on the distance of closest approach to the volcano. These statistical analyses provide information about the emission height time series of SO2 injection from that eruption. It is found that the eruption begins first injecting SO2 into the upper troposphere, between 13 km and 17 km, on November 28th 2006. This is then followed by a slow decay in injection altitude, down to 6 km, over subsequent days. The emission height profile is used to generate an optimal reconstruction based on forward trajectories and compared to OMI SO2 observations. The inferred altitude of the Nyamuragira SO2 cloud is also compared to the altitude of sulfate aerosols detected in aerosol backscatter vertical profiles from the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) instrument aboard the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO).
C1 [Hughes, E. J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Hughes, E. J.; Sparling, L. C.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA.
[Carn, S. A.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA.
[Krueger, A. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hughes, EJ (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM ehughes@atmos.umd.edu
FU NAS [NNX07AD87G]; U.S. National Science Foundation [EAR 0910795]
FX The authors wish to thank Mark Schoeberl for his work on the trajectory
model used in this study. This study was supported by NASA under grant
NNX07AD87G and by the U.S. National Science Foundation under grant EAR
0910795.
NR 23
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Z9 9
U1 1
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 27
PY 2012
VL 117
AR D18307
DI 10.1029/2012JD017957
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 015AU
UT WOS:000309418000001
ER
PT J
AU Ghimire, B
Williams, CA
Collatz, GJ
Vanderhoof, M
AF Ghimire, Bardan
Williams, Christopher A.
Collatz, G. James
Vanderhoof, Melanie
TI Fire-induced carbon emissions and regrowth uptake in western U.S.
forests: Documenting variation across forest types, fire severity, and
climate regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID MIXED-CONIFER FOREST; NORTHERN ROCKY-MOUNTAINS; ECOSYSTEM CO2 EXCHANGE;
PONDEROSA PINE FORESTS; NET PRIMARY PRODUCTION; COMPOSITE BURN INDEX;
TREE MORTALITY; SIERRA-NEVADA; PRESCRIBED-FIRE; BOREAL FOREST
AB The forest area in the western United States that burns annually is increasing with warmer temperatures, more frequent droughts, and higher fuel densities. Studies that examine fire effects for regional carbon balances have tended to either focus on individual fires as examples or adopt generalizations without considering how forest type, fire severity, and regional climate influence carbon legacies. This study provides a more detailed characterization of fire effects and quantifies the full carbon impacts in relation to direct emissions, slow release of fire-killed biomass, and net carbon uptake from forest regrowth. We find important variations in fire-induced mortality and combustion across carbon pools (leaf, live wood, dead wood, litter, and duff) and across low- to high-severity classes. This corresponds to fire-induced direct emissions from 1984 to 2008 averaging 4 TgC yr(-1) and biomass killed averaging 10.5 TgC yr(-1), with average burn area of 2723 km(2) yr(-1) across the western United States. These direct emission and biomass killed rates were 1.4 and 3.7 times higher, respectively, for high-severity fires than those for low- severity fires. The results show that forest regrowth varies greatly by forest type and with severity and that these factors impose a sustained carbon uptake legacy. The western U.S. fires between 1984 and 2008 imposed a net source of 12.3 TgC yr(-1) in 2008, accounting for both direct fire emissions (9.5 TgC yr(-1)) and heterotrophic decomposition of fire-killed biomass (6.1 TgC yr(-1)) as well as contemporary regrowth sinks (3.3 TgC yr(-1)). A sizeable trend exists toward increasing emissions as a larger area burns annually.
C1 [Ghimire, Bardan; Williams, Christopher A.; Vanderhoof, Melanie] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA.
[Collatz, G. James] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
RP Ghimire, B (reprint author), Clark Univ, Grad Sch Geog, 950 Main St, Worcester, MA 01610 USA.
EM bghimire@clarku.edu
RI collatz, george/D-5381-2012; Ghimire, Bardan/N-9871-2013
FU NASA Terrestrial Ecology program [NNX10AR68G]
FX The authors would like to thank the Editor and two anonymous reviewers
for constructive comments that improved the manuscript. The authors are
grateful to Andy Youngblood (USDA Forest Service, Pacific Northwest
Research Station), Carolyn Hull Sieg (USDA Forest Service, Rocky
Mountain Research Station), Chuck McHugh (USDA Forest Service, Rocky
Mountain Research Station), Clint Wright (USDA Forest Service, Pacific
Northwest Research Station), Eric E. Knapp (USDA Forest Service, Pacific
Southwest Research Station), James K. Agee (University of Washington,
Seattle), Kevin C. Ryan (USDA Forest Service, Rocky Mountain Research
Station), Kostas D. Kalabokidis (University of the Aegean, Mytilene),
Leda Kobziar (University of Florida, Gainesville), Malcolm North (USDA
Forest Service, Pacific Southwest Research Station), Nicole Vaillant
(USDA Forest Service, Pacific Northwest Research Station), Peter Z. Fule
(Northern Arizona University, Flagstaff), Phillip van Mantgem (USGS,
Western Ecological Research Center), Scott L. Stephens (University of
California, Berkeley), Sharon M. Hood (USDA Forest Service, Rocky
Mountain Research Station), Tara Keyser (USDA Forest Service, Southern
Research Station), and Walter G. Thies (USDA Forest Service, Pacific
Northwest Research Station) for participating in the severity assessment
survey. B.G., C.A.W. and G.J.C. thank the NASA Terrestrial Ecology
program for financial support under grant NNX10AR68G.
NR 89
TC 15
Z9 15
U1 1
U2 41
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD SEP 27
PY 2012
VL 117
AR G03036
DI 10.1029/2011JG001935
PG 29
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 015AC
UT WOS:000309416100001
ER
PT J
AU He, MS
Vogt, J
Luhr, H
Sorbalo, E
Blagau, A
Le, G
Lu, G
AF He, Maosheng
Vogt, Joachim
Luehr, Hermann
Sorbalo, Eugen
Blagau, Adrian
Le, Guan
Lu, Gang
TI A high-resolution model of field-aligned currents through empirical
orthogonal functions analysis (MFACE)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; IONOSPHERIC ELECTRIC-FIELDS; DAYSIDE
CUSP; SATELLITE; CONSTELLATION; POTENTIALS; SATURATION; SUBSTORMS;
REGION; MAPS
AB Ten years of CHAMP magnetic field measurements are integrated into MFACE, a model of field-aligned currents (FACs) using empirical orthogonal functions (EOFs). EOF1 gives the basic Region-1/Region-2 pattern varying mainly with the interplanetary magnetic field Bz component. EOF2 captures separately the cusp current signature and By-related variability. Compared to existing models, MFACE yields significantly better spatial resolution, reproduces typically observed FAC thickness and intensity, improves on the magnetic local time (MLT) distribution, and gives the seasonal dependence of FAC latitudes and the NBZ current signature. MFACE further reveals systematic dependences on By, including 1) Region-1/Region-2 topology modifications around noon; 2) imbalance between upward and downward maximum current density; 3) MLT location of the Harang discontinuity. Furthermore, our procedure allows quantifying response times of FACs to solar wind driving at the bow shock nose: we obtain 20 minutes and 35-40 minutes lags for the FAC density and latitude, respectively. Citation: He, M., J. Vogt, H. Luhr, E. Sorbalo, A. Blagau, G. Le, and G. Lu (2012), A high-resolution model of field-aligned currents through empirical orthogonal functions analysis (MFACE), Geophys. Res. Lett., 39, L18105, doi:10.1029/2012GL053168.
C1 [He, Maosheng; Vogt, Joachim; Sorbalo, Eugen; Blagau, Adrian] Jacobs Univ Bremen, Sch Sci & Engn, D-28759 Bremen, Germany.
[Luehr, Hermann] Deutsch GeoForschungsZentrum Potsdam, Potsdam, Germany.
[Blagau, Adrian] Inst Space Sci, Bucharest, Romania.
[Le, Guan] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Lu, Gang] NCAR, High Altitude Observ, Boulder, CO USA.
RP He, MS (reprint author), Jacobs Univ Bremen, Sch Sci & Engn, Campus Ring 1, D-28759 Bremen, Germany.
EM m.he@jacobs.university.de
RI Le, Guan/C-9524-2012; He, Maosheng/G-6913-2012; Lu, Gang/A-6669-2011
OI Le, Guan/0000-0002-9504-5214; He, Maosheng/0000-0001-6112-2499;
FU DFG [VO 855/3-1]
FX The authors thank Boris Prokhorov, Patricia Ritter and Stefan Maus for
their help, and acknowledge the online services provided by GFZ Potsdam
(CHAMP data), NGDC (POMME-6.2 coefficients), John Hopkins University APL
(AACGM coefficients), and NASA OMNI (IMF/SW and other geophysical
parameters). The MFACE code would be released through the link
www.faculty.jacobs-university.de/jvogt/mface/ and Source Forge. This
work is supported by DFG grant VO 855/3-1.
NR 31
TC 22
Z9 22
U1 2
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 26
PY 2012
VL 39
AR L18105
DI 10.1029/2012GL053168
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 014ZO
UT WOS:000309414700005
ER
PT J
AU Petrenko, M
Kahn, R
Chin, M
Soja, A
Kucsera, T
Harshvardhan
AF Petrenko, Mariya
Kahn, Ralph
Chin, Mian
Soja, Amber
Kucsera, Tom
Harshvardhan
TI The use of satellite-measured aerosol optical depth to constrain biomass
burning emissions source strength in the global model GOCART
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SUN PHOTOMETER MEASUREMENTS; LAND-COVER PRODUCTS; AIR-QUALITY;
NORTH-AMERICA; BURNED AREA; FIRE EMISSIONS; HAINES INDEX; TRANSPORT;
FOREST; IMPACT
AB Simulations of biomass burning (BB) emissions in chemistry transport models strongly depend on the inventories that define emission source location and strength. We use 13 global biomass burning emission estimates, including the widely used Global Fire Emission Database (GFED) monthly and daily versions, Fire Radiative Power (FRP)-based Quick Fire Emission Data set QFED, and 11 calculated emissions from different combinations of burned area based on the Moderate Resolution Imaging Spectroradiometer (MODIS) products, effective fuel load, and species emission factors as alternative inputs to the global Goddard Chemistry Aerosol Radiation and Transport (GOCART) model. The resultant simulated aerosol optical depth (AOD) and its spatial distribution are compared to AOD snapshots measured by the MODIS instrument for 124 fire events occurring between 2006 and 2007. This comparison exposes the regional biases of each emission option. GOCART average fire AOD values compare best to MODIS-measured AOD when the daily GFED inventory is used as input to GOCART. Even though GFED-based emission options provide the lowest emissions in the tropics, GFED-based GOCART AOD compares best with MODIS AOD in tropical cases. Fire-counts-based emission options give the largest emission estimates in the boreal regions, and the model performs best at higher latitudes with these inputs when compared to MODIS. Comparison of total annual BB emissions by all inventories suggests that burned area estimates are usually the largest source of disagreement. It is also shown that the quantitative relationship between BB aerosol emission rate and model-simulated AOD is related to the horizontal plume dispersion, which can be approximated by the wind speed in the planetary boundary layer in most cases. Thus, given average wind speed of the smoke plume environment, MODIS-measured AOD can provide a constraint to the strength of BB sources at the level of individual plumes.
C1 [Petrenko, Mariya; Kahn, Ralph; Chin, Mian; Kucsera, Tom] NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA.
[Petrenko, Mariya; Harshvardhan] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
[Petrenko, Mariya] USRA, Columbia, MD USA.
[Soja, Amber] Natl Inst Aerosp, Hampton, VA USA.
[Soja, Amber] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Kucsera, Tom] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Petrenko, M (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Code 613, Greenbelt, MD 20771 USA.
EM mshcherb@purdue.edu
RI Chin, Mian/J-8354-2012; Kahn, Ralph/D-5371-2012
OI Kahn, Ralph/0000-0002-5234-6359
FU NASA [NNX08AU81H, NNX10AG61G]; NASA's Atmospheric Composition Program;
NASA's Climate and Radiation Research and Analysis Program; EOS MISR
project
FX We thank Catherine Liousse for providing GLC2000 effective fuel load
files and emission factors, Anton Darmenov and Arlindo da Silva for
providing access to QFED emission data set, Matthew Davis and James
Limbacher for software support when processing satellite data products,
and Thomas Diehl and Qian Tan for help with configuring the GOCART
model. We thank the reviewers for providing very useful and insightful
comments, that helped improve this manuscript. This work was funded
primarily by NASA grants NNX08AU81H and NNX10AG61G to Purdue University.
The work of R. Kahn is supported in part by NASA's Atmospheric
Composition Program, NASA's Climate and Radiation Research and Analysis
Program under H. Maring, and the EOS MISR project.
NR 98
TC 25
Z9 25
U1 3
U2 34
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 26
PY 2012
VL 117
AR D18212
DI 10.1029/2012JD017870
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 015AR
UT WOS:000309417700003
ER
PT J
AU Yuan, TL
Remer, LA
Bian, HS
Ziemke, JR
Albrecht, R
Pickering, KE
Oreopoulos, L
Goodman, SJ
Yu, HB
Allen, DJ
AF Yuan, Tianle
Remer, Lorraine A.
Bian, Huisheng
Ziemke, Jerald R.
Albrecht, Rachel
Pickering, Kenneth E.
Oreopoulos, Lazaros
Goodman, Steven J.
Yu, Hongbin
Allen, Dale J.
TI Aerosol indirect effect on tropospheric ozone via lightning
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL TRANSIENT DETECTOR; DEEP CONVECTIVE CLOUDS; GLOBAL-MODEL;
PREINDUSTRIAL TIMES; ACCURATE SIMULATION; CHEMICAL-MODELS;
UNITED-STATES; NORTH-AMERICA; WAVE-ONE; NOX
AB Tropospheric ozone (O-3) is a pollutant and major greenhouse gas and its radiative forcing is still uncertain. Inadequate understanding of processes related to O-3 production, in particular those natural ones such as lightning, contributes to this uncertainty. Here we demonstrate a new effect of aerosol particles on O-3 production by affecting lightning activity and lightning-generated NOx (LNOx). We find that lightning flash rate increases at a remarkable rate of 30 times or more per unit of aerosol optical depth. We provide observational evidence that indicates the observed increase in lightning activity is caused by the influx of aerosols from a volcano. Satellite data analyses show O-3 is increased as a result of aerosol-induced increase in lightning and LNOx, which is supported by modle simulations with prescribed lightning change. O-3 production increase from this aerosol-lightning-ozone link is concentrated in the upper troposphere, where O-3 is most efficient as a greenhouse gas. In the face of anthropogenic aerosol increase our findings suggest that lightning activity, LNOx and O-3, especially in the upper troposphere, have all increased substantially since preindustrial time due to the proposed aerosol-lightning-ozone link, which implies a stronger O-3 historical radiative forcing. Aerosol forcing therefore has a warming component via its effect on O-3 production and this component has mostly been ignored in previous studies of climate forcing related to O-3 and aerosols. Sensitivity simulations suggest that 4-8% increase of column tropospheric ozone, mainly in the tropics, is expected if aerosol-lighting-ozone link is parameterized, depending on the background emission scenario. We note, however, substantial uncertainties remain on the exact magnitude of aerosol effect on tropospheric O-3 via lightning. The challenges for obtaining a quantitative global estimate of this effect are also discussed. Our results have significant implications for understanding past and projecting future tropospheric O-3 forcing as well as wildfire changes and call for integrated investigations of the coupled aerosol-cloud-chemistry system.
C1 [Yuan, Tianle; Oreopoulos, Lazaros; Yu, Hongbin] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
[Yuan, Tianle; Remer, Lorraine A.; Bian, Huisheng] Univ Maryland Baltimore Cty, Joint Ctr Environm Technol, Baltimore, MD 21228 USA.
[Bian, Huisheng; Ziemke, Jerald R.; Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Ziemke, Jerald R.] Morgan State Univ, Baltimore, MD 21239 USA.
[Albrecht, Rachel] DSA CPTEC, Inst Nacl Pesquisas Espaciais, Cachoeira Paulista, Brazil.
[Goodman, Steven J.] NASA, Goddard Space Flight Ctr, NOAA NESDIS, Greenbelt, MD 20771 USA.
[Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Allen, Dale J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP Yuan, TL (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Bldg 33,Room A306, Greenbelt, MD 20771 USA.
EM tianle.yuan@nasa.gov
RI Oreopoulos, Lazaros/E-5868-2012; Yu, Hongbin/C-6485-2008; Yuan,
Tianle/D-3323-2011; Albrecht, Rachel/D-9311-2012; Pickering,
Kenneth/E-6274-2012; Allen, Dale/F-7168-2010
OI Oreopoulos, Lazaros/0000-0001-6061-6905; Yu,
Hongbin/0000-0003-4706-1575; Albrecht, Rachel/0000-0003-0582-6568;
Allen, Dale/0000-0003-3305-9669
FU NASA Earth Observing System; TRMM Lightning Imaging Sensor Instrument
team; NOAA GOES-R Geostationary Lightning Mapper science team; NASA's
IDS program; NASA's Radiation Science program
FX We thank three anonymous reviewers for their constructive suggestions to
improve our manuscript. We acknowledge the free use of tropospheric
NO2 column data from the various groups including OMI, GOME,
SCIAMARCHY from www.temis.nl; Randall Martin's group from
http://fizz.phys.dal.ca/similar to atmos/g47.swf; and the University of
Bremen group from http://www.iup.uni-bremen.de/doas/index.html. The LIS
data set and associated analysis were in part supported by the NASA
Earth Observing System, the TRMM Lightning Imaging Sensor Instrument
team, and the NOAA GOES-R Geostationary Lightning Mapper science team.
The LIS data are available from the NASA EOSDIS Global Hydrology
Resource Center DAAC, Huntsville, Alabama, USA,
http://thunder.nsstc.nasa.gov. We would also acknowledge funding support
for this work by NASA's IDS and Radiation Science programs.
NR 90
TC 12
Z9 12
U1 3
U2 34
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 26
PY 2012
VL 117
AR D18213
DI 10.1029/2012JD017723
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 015AR
UT WOS:000309417700001
ER
PT J
AU Yoon, Y
Durand, M
Merry, CJ
Clark, EA
Andreadis, KM
Alsdorf, DE
AF Yoon, Yeosang
Durand, Michael
Merry, Carolyn J.
Clark, Elizabeth A.
Andreadis, Konstantinos M.
Alsdorf, Douglas E.
TI Estimating river bathymetry from data assimilation of synthetic SWOT
measurements
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE SWOT; Hydrologic/hydraulic modeling; Data assimilation; Ensemble Kalman
Filter; River bathymetry; River discharge
ID ENSEMBLE KALMAN FILTER; HYDRAULIC MODELS; SURFACE-WATER; DISCHARGE;
ERROR; ALTIMETRY; FLUXES; STATES
AB This paper focuses on estimating river bathymetry for retrieving river discharge from the upcoming Surface Water and Ocean Topography (SWOT) satellite mission using a data assimilation algorithm coupled with a hydrodynamic model. The SWOT observations will include water surface elevation (WSE), its spatial and temporal derivatives, and inundated area. We assimilated synthetic SWOT observations into the LISFLOOD-FP hydrodynamic model using a local ensemble batch smoother (LEnBS), simultaneously estimating river bathymetry and flow depth. SWOT observations were obtained by sampling a "true" LISFLOOD-FP simulation based on the SWOT instrument design; the "true" discharge boundary condition was derived from USGS gages. The first-guess discharge boundary conditions were produced by the Variable Infiltration Capacity model, with discharge uncertainty controlled via precipitation uncertainty. First-guess estimates of bathymetry were derived from SWOT observations assuming a uniform spatial depth; bathymetric variability was modeled using an exponential correlation function. Thus, discharge and bathymetry errors were modeled realistically. The LEnBS recovered the bathymetry from SWOT observations with 0.52 m reach-average root mean square error (RMSE), which was 67.8% less than the first-guess RMSE. The RMSE of bathymetry estimates decreased sequentially as more SWOT observations were used in the estimate; we illustrate sequential processing of 6 months of SWOT observations. The better estimates of bathymetry lead to improved discharge estimates. The normalized RMSE of the river discharge estimates was 10.5%, 71.2% less than the first-guess error. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Yoon, Yeosang; Merry, Carolyn J.] Ohio State Univ, Dept Civil Environm & Geodet Engn, Columbus, OH 43210 USA.
[Durand, Michael; Alsdorf, Douglas E.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Yoon, Yeosang; Durand, Michael; Merry, Carolyn J.; Alsdorf, Douglas E.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Clark, Elizabeth A.] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA.
[Andreadis, Konstantinos M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yoon, Y (reprint author), Ohio State Univ, Dept Civil Environm & Geodet Engn, 470 Hitchcock Hall,2070 Neil Ave, Columbus, OH 43210 USA.
EM yoon.203@osu.edu; durand.8@osu.edu; merry.1@osu.edu;
eclark@hydro.washington.edu; konstantinos.m.andreadis@jpl.nasa.gov;
alsdorf.1@osu.edu
RI Durand, Michael/D-2885-2013
FU Ohio State University Climate, Water and Carbon program; NASA Physical
Oceanography Grant [NNX10AE96G]; NASA Headquarters under the NASA Earth
and Space Science Fellowship Program-Grant [NNX11AL60H]; Ohio
Supercomputer Center [PAS0503]
FX This work was partially supported by The Ohio State University Climate,
Water and Carbon program, NASA Physical Oceanography Grant NNX10AE96G,
and NASA Headquarters under the NASA Earth and Space Science Fellowship
Program-Grant NNX11AL60H. The authors would like to thank Trent Schade
and Deborah Lee at the U.S. Army Corps of Engineers, Ohio River
Division, Cincinnati, Ohio for the bathymetric data of the Ohio River.
Computational support for this project was provided by the Ohio
Supercomputer Center, under Project PAS0503.
NR 51
TC 24
Z9 24
U1 0
U2 48
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
EI 1879-2707
J9 J HYDROL
JI J. Hydrol.
PD SEP 25
PY 2012
VL 464
BP 363
EP 375
DI 10.1016/j.jhydrol.2012.07.028
PG 13
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 020BN
UT WOS:000309783700028
ER
PT J
AU Ho, SP
Hunt, D
Steiner, AK
Mannucci, AJ
Kirchengast, G
Gleisner, H
Heise, S
von Engeln, A
Marquardt, C
Sokolovskiy, S
Schreiner, W
Scherllin-Pirscher, B
Ao, C
Wickert, J
Syndergaard, S
Lauritsen, KB
Leroy, S
Kursinski, ER
Kuo, YH
Foelsche, U
Schmidt, T
Gorbunov, M
AF Ho, Shu-peng
Hunt, Doug
Steiner, Andrea K.
Mannucci, Anthony J.
Kirchengast, Gottfried
Gleisner, Hans
Heise, Stefan
von Engeln, Axel
Marquardt, Christian
Sokolovskiy, Sergey
Schreiner, William
Scherllin-Pirscher, Barbara
Ao, Chi
Wickert, Jens
Syndergaard, Stig
Lauritsen, Kent B.
Leroy, Stephen
Kursinski, Emil R.
Kuo, Ying-Hwa
Foelsche, Ulrich
Schmidt, Torsten
Gorbunov, Michael
TI Reproducibility of GPS radio occultation data for climate monitoring:
Profile-to-profile inter-comparison of CHAMP climate records 2002 to
2008 from six data centers
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATMOSPHERIC PROFILES; ERROR ESTIMATION; STATISTICAL OPTIMIZATION;
IONOSPHERIC CORRECTION; TEMPERATURE RECORDS; NEUTRAL ATMOSPHERE; BENDING
ANGLES; SATELLITE; SYSTEM; REFRACTIVITY
AB To examine the claim that Global Positioning System (GPS) radio occultation (RO) data are useful as a benchmark data set for climate monitoring, the structural uncertainties of retrieved profiles that result from different processing methods are quantified. Profile-to-profile comparisons of CHAMP (CHAllenging Minisatellite Payload) data from January 2002 to August 2008 retrieved by six RO processing centers are presented. Differences and standard deviations of the individual centers relative to the inter-center mean are used to quantify the structural uncertainty. Uncertainties accumulate in derived variables due to propagation through the RO retrieval chain. This is reflected in the inter-center differences, which are small for bending angle and refractivity increasing to dry temperature, dry pressure, and dry geopotential height. The mean differences of the time series in the 8 km to 30 km layer range from -0.08% to 0.12% for bending angle, -0.03% to 0.02% for refractivity, -0.27 K to 0.15 K for dry temperature, -0.04% to 0.04% for dry pressure, and -7.6 m to 6.8 m for dry geopotential height. The corresponding standard deviations are within 0.02%, 0.01%, 0.06 K, 0.02%, and 2.0 m, respectively. The mean trend differences from 8 km to 30 km for bending angle, refractivity, dry temperature, dry pressure, and dry geopotential height are within +/- 0.02%/5 yrs, +/- 0.02%/5 yrs, +/- 0.06 K/5 yrs, +/- 0.02%/5 yrs, and +/- 2.3 m/5 yrs, respectively. Although the RO-derived variables are not readily traceable to the international system of units, the high precision nature of the raw RO observables is preserved in the inversion chain.
C1 [Ho, Shu-peng; Hunt, Doug; Sokolovskiy, Sergey; Schreiner, William; Kuo, Ying-Hwa] Univ Corp Atmospheric Res, COSMIC Project Off, Boulder, CO 80307 USA.
[Steiner, Andrea K.; Kirchengast, Gottfried; Scherllin-Pirscher, Barbara; Foelsche, Ulrich] Graz Univ, Wegener Ctr Climate & Global Change, Graz, Austria.
[Steiner, Andrea K.; Kirchengast, Gottfried; Scherllin-Pirscher, Barbara; Foelsche, Ulrich] Graz Univ, Inst Geophys Astrophys & Meteorol, Inst Phys, Graz, Austria.
[Mannucci, Anthony J.; Ao, Chi] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Gleisner, Hans; Syndergaard, Stig; Lauritsen, Kent B.; Gorbunov, Michael] Danish Meteorol Inst, Copenhagen, Denmark.
[Heise, Stefan; Wickert, Jens; Schmidt, Torsten] German Res Ctr Geosci, Dept Geodesy & Remote Sensing, Potsdam, Germany.
[von Engeln, Axel; Marquardt, Christian] EUMETSAT, Darmstadt, Germany.
[Leroy, Stephen] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Kursinski, Emil R.] Univ Arizona, Inst Atmospher Phys, Tucson, AZ 85721 USA.
[Gorbunov, Michael] Russian Acad Sci, Inst Atmospher Phys, Moscow, Russia.
RP Ho, SP (reprint author), Univ Corp Atmospheric Res, COSMIC Project Off, POB 3000, Boulder, CO 80307 USA.
EM spho@ucar.edu
RI Schmidt, Torsten/A-7142-2013; Wickert, Jens/A-7257-2013; Kirchengast,
Gottfried/D-4990-2016; Syndergaard, Stig/C-1103-2017; Heise,
Stefan/K-2190-2013
OI Schmidt, Torsten/0000-0001-9302-1000; Kirchengast,
Gottfried/0000-0001-9187-937X; Syndergaard, Stig/0000-0003-3119-2618;
Foelsche, Ulrich/0000-0002-9899-6453;
FU Radio Occultation Meteorology Satellite Application Facility under
EUMETSAT; ERA-CLIM project European Commission; GEOTECHNOLOGIEN
[03G0728A]; National Aeronautics and Space Administration; National
Science Foundation [AGS-0918398/CSA, AGS-0939962]; NOAA
[NA07OAR4310224]; Austrian Science Fund (FWF) [P21642-N21, P22293-N21];
European Space Agency; FFG-ALR Austria
FX We thank all the scientists, engineers and technicians of the CHAMP
satellite mission for their successful work, which is the basis for our
investigations. The DMI work was supported by the Radio Occultation
Meteorology (formerly GRAS) Satellite Application Facility, which is an
operational RO processing center under EUMETSAT. DMI thanks K. R. Larsen
for assistance in the processing of data. The work of EUM was partially
funded by the ERA-CLIM project, under the Seventh Framework Programme
for Research and Technological Development of the European Commission
(FP7). The work of GFZ was supported by GEOTECHNOLOGIEN grant 03G0728A.
The work of JPL, California Institute of Technology, was carried out
under a contract with the National Aeronautics and Space Administration.
The work of UCAR was supported by the National Science Foundation under
cooperative agreement AGS-0918398/CSA AGS-0939962. The National Center
for Atmospheric Research is sponsored by the National Science
Foundation. Shu-peng Ho acknowledges NOAA support under grant
NA07OAR4310224. The work of WEGC was funded by the Austrian Science Fund
(FWF) grants P21642-N21 and P22293-N21 and partially by European Space
Agency and FFG-ALR Austria contracts.
NR 85
TC 37
Z9 37
U1 2
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 25
PY 2012
VL 117
AR D18111
DI 10.1029/2012JD017665
PG 38
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 015AJ
UT WOS:000309416800002
ER
PT J
AU LeBlanc, SE
Schmidt, KS
Pilewskie, P
Redemann, J
Hostetler, C
Ferrare, R
Hair, J
Langridge, JM
Lack, DA
AF LeBlanc, Samuel E.
Schmidt, K. S.
Pilewskie, P.
Redemann, J.
Hostetler, C.
Ferrare, R.
Hair, J.
Langridge, J. M.
Lack, D. A.
TI Spectral aerosol direct radiative forcing from airborne radiative
measurements during CalNex and ARCTAS
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL-PROPERTIES; COMPREHENSIVE CHARACTERIZATION; AIRCRAFT INSTRUMENT;
INDIAN-OCEAN; DEPTH; SPECTROSCOPY; VARIABILITY; ABSORPTION; ATMOSPHERE;
DEPENDENCE
AB This study presents the aerosol radiative forcing derived from airborne measurements of shortwave spectral irradiance during the 2010 Research at the Nexus of Air Quality and Climate Change (CalNex). Relative forcing efficiency, the radiative forcing normalized by aerosol optical thickness and incident irradiance, is a means of comparing the aerosol radiative forcing for different conditions. In this study, it is used to put the aerosol radiative effects of an air mass in the Los Angeles basin in context with case studies from three field missions that targeted other regions and aerosol types, including a case study from the Arctic Research of the Composition of the Troposphere from Aircraft and Satellites (ARCTAS). For CalNex, we relied on irradiance measurements onboard the NOAA P-3 aircraft during a flight on 19 May 2010 over a ground station. CalNex presented a difficulty for determining forcing efficiency since one of the input parameters, optical thickness, was not available from the same aircraft. However, extinction profiles were available from a nearby aircraft. An existing retrieval algorithm was modified to use those measurements as initial estimate for the missing optical thickness. In addition, single scattering albedo and asymmetry parameter (secondary products of the method), were compared with CalNex in situ measurements. The CalNex relative forcing efficiency spectra agreed with earlier studies that found this parameter to be constrained at each wavelength within 20% per unit of aerosol optical thickness at 500 nm regardless of aerosol type and experiment, except for highly absorbing aerosols sampled near Mexico City. The diurnally averaged below-layer forcing efficiency integrated over the wavelength range of 350-700 nm for CalNex is estimated to be -58.6 +/- 13.8 W/m(2), whereas for the ARCTAS case it is -48.7 +/- 11.5 W/m(2).
C1 [LeBlanc, Samuel E.; Pilewskie, P.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[LeBlanc, Samuel E.; Schmidt, K. S.; Pilewskie, P.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Redemann, J.] Bay Area Environm Res Inst, Sonoma, CA USA.
[Hostetler, C.; Ferrare, R.; Hair, J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Langridge, J. M.; Lack, D. A.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA.
[Langridge, J. M.; Lack, D. A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
RP LeBlanc, SE (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, 311 UCB,Rm 255,Gate 7, Boulder, CO 80309 USA.
EM samuel.leblanc@colorado.edu
RI Lack, Daniel/I-9053-2012; SCHMIDT, KONRAD SEBASTIAN/C-1258-2013;
LeBlanc, Samuel/F-1150-2013; Manager, CSD Publications/B-2789-2015
OI SCHMIDT, KONRAD SEBASTIAN/0000-0003-3899-228X; LeBlanc,
Samuel/0000-0003-0173-3890;
FU NOAA CalNex [NA06OAR4310085]; NASA ARCTAS [NNX08AF93G]; NASA HQ Science
Mission Directorate Radiation Sciences Program; NASA CALIPSO project;
Department of Energy's Atmospheric Science Program Atmospheric System
Research, an Office of Science, Office of Biological and Environmental
Research program [DE-AI02-05ER63985]
FX This work was supported through NOAA CalNex (grant NA06OAR4310085) and
NASA ARCTAS (grant NNX08AF93G). The authors would like to recognize the
efforts from Warren Gore and Antony Trias from NASA Ames for their
continued and reliable support of the SSFR during these deployments. We
thank the NASA Langley B200 King Air and NOAA WP-3D flight crews for
their outstanding work in support of these measurements. Support for the
HSRL measurements came from the NASA HQ Science Mission Directorate
Radiation Sciences Program, the NASA CALIPSO project, and the Department
of Energy's Atmospheric Science Program Atmospheric System Research, an
Office of Science, Office of Biological and Environmental Research
program, under grant DE-AI02-05ER63985.
NR 38
TC 3
Z9 3
U1 0
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 25
PY 2012
VL 117
AR D00V20
DI 10.1029/2012JD018106
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 015AJ
UT WOS:000309416800006
ER
PT J
AU Petrich, C
Eicken, H
Polashenski, CM
Sturm, M
Harbeck, JP
Perovich, DK
Finnegan, DC
AF Petrich, Chris
Eicken, Hajo
Polashenski, Christopher M.
Sturm, Matthew
Harbeck, Jeremy P.
Perovich, Donald K.
Finnegan, David C.
TI Snow dunes: A controlling factor of melt pond distribution on Arctic sea
ice
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID ALBEDO; VARIABILITY; EVOLUTION; OCEAN; DEPTH
AB The location of snow dunes over the course of the ice-growth season 2007/08 was mapped on level landfast first-year sea ice near Barrow, Alaska. Landfast ice formed in mid-December and exhibited essentially homogeneous snow depths of 4-6 cm in mid-January; by early February distinct snow dunes were observed. Despite additional snowfall and wind redistribution throughout the season, the location of the dunes was fixed by March, and these locations were highly correlated with the distribution of meltwater ponds at the beginning of June. Our observations, including ground-based light detection and ranging system (lidar) measurements, show that melt ponds initially form in the interstices between snow dunes, and that the outline of the melt ponds is controlled by snow depth contours. The resulting preferential surface ablation of ponded ice creates the surface topography that later determines the melt pond evolution.
C1 [Petrich, Chris] No Res Inst, NO-8504 Narvik, Norway.
[Petrich, Chris; Eicken, Hajo; Harbeck, Jeremy P.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Eicken, Hajo] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK USA.
[Polashenski, Christopher M.; Sturm, Matthew] USA, Cold Reg Res & Engn Lab Alaska, Ft Wainwright, AK USA.
[Harbeck, Jeremy P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Perovich, Donald K.; Finnegan, David C.] USA, Cold Reg Res & Engn Lab, Hanover, NH 03755 USA.
RP Petrich, C (reprint author), No Res Inst, POB 250, NO-8504 Narvik, Norway.
EM christian.petrich@norut.no
RI Eicken, Hajo/M-6901-2016;
OI Petrich, Chris/0000-0003-2226-0789
FU National Science Foundation Office of Polar Programs [OPP-0632398,
OPP-0856867]; University of Alaska Foundation; Research Council of
Norway [195153]
FX Data acquisition for this project was supported by the National Science
Foundation Office of Polar Programs (awards OPP-0632398 and
OPP-0856867). Chris Petrich would like to acknowledge an International
Polar Year postdoctoral fellowship of the University of Alaska
Foundation and the Research Council of Norway (project number 195153)
that allowed for analysis of the data. Weather data were provided by the
National Oceanic and Atmospheric Administration (NOAA). We wish to
acknowledge staff at the Barrow Arctic Science Consortium (BASC) for
excellent support of this project. Magnaprobe snow depth measurements on
1 May 2008 and some thickness measurements for Figure 6 were performed
by volunteers of Ben and Jerry's Climate Change College. We are indebted
to Martin Stuefer for providing us with the opportunity to take aerial
photographs from his plane. The constructive comments of Ian Eisenman
and two anonymous reviewers of an earlier version of this manuscript,
and two anonymous reviewers of this manuscript are gratefully
acknowledged.
NR 33
TC 18
Z9 19
U1 1
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD SEP 25
PY 2012
VL 117
AR C09029
DI 10.1029/2012JC008192
PG 10
WC Oceanography
SC Oceanography
GA 015BW
UT WOS:000309421000001
ER
PT J
AU Cutler, C
AF Cutler, Curt
TI An improved, "phase-relaxed" F-statistic for gravitational-wave data
analysis
SO PHYSICAL REVIEW D
LA English
DT Article
AB Rapidly rotating, slightly nonaxisymmetric neutron stars emit nearly periodic gravitational waves (GWs), quite possibly at levels detectable by ground-based GW interferometers. We refer to these sources as "GW pulsars." For any given sky position and frequency evolution, the F-statistic is the maximum likelihood statistic for the detection of GW pulsars. However, in "all-sky" searches for previously unknown GW pulsars, it would be computationally intractable to calculate the (fully coherent) F-statistic at every point of (a suitably fine) grid covering the parameter space: the number of grid points is many orders of magnitude too large for that. Therefore, in practice some nonoptimal detection statistic is used for all-sky searches. Here we introduce a "phase-relaxed" F-statistic, which we denote F-pr, for incoherently combining the results of fully coherent searches over short time intervals. We estimate (very roughly) that for realistic searches, our F-pr is similar to 10-15% more sensitive than the "semicoherent" F-statistic that is currently used. Moreover, as a by-product of computing F-pr, one obtains a rough determination of the time-evolving phase offset between one's template and the true signal imbedded in the detector noise. Almost all the ingredients that go into calculating F-pr are already implemented in the LIGO Algorithm Library, so we expect that relatively little additional effort would be required to develop a search code that uses F-pr.
C1 [Cutler, Curt] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cutler, Curt] CALTECH, Pasadena, CA 91125 USA.
RP Cutler, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU NSF Grant [PHY-0601459]
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract to the National Aeronautics and
Space Administration. We gratefully acknowledge support from NSF Grant
No. PHY-0601459. We also thank Michele Vallisneri, Holger Pletsch,
Reinhard Prix, Badri Krishnan, and Bruce Allen for helpful discussions.
NR 14
TC 2
Z9 2
U1 0
U2 0
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 SEP 25
PY 2012
VL 86
IS 6
AR 063012
DI 10.1103/PhysRevD.86.063012
PG 8
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 011UP
UT WOS:000309191100001
ER
PT J
AU Bhatia, AK
AF Bhatia, A. K.
TI Application of P-wave hybrid theory to the scattering of electrons from
He+ and resonances in He and H-
SO PHYSICAL REVIEW A
LA English
DT Article
ID PHASE-SHIFTS; THRESHOLDS; STATES; N=2
AB The P-wave hybrid theory of electron-hydrogen elastic scattering [Bhatia, Phys. Rev. A 85, 052708 (2012)] is applied to the P-wave scattering from He ion. In this method, both short-range and long-range correlations are included in the Schrodinger equation at the same time, by using a combination of a modified method of polarized orbitals and the optical potential formalism. The short-range-correlation functions are of Hylleraas type. It is found that the phase shifts are not significantly affected by the modification of the target function by a method similar to the method of polarized orbitals and they are close to the phase shifts calculated earlier by Bhatia [Phys. Rev. A 69, 032714 (2004)]. This indicates that the correlation function is general enough to include the target distortion (polarization) in the presence of the incident electron. The important fact is that in the present calculation, to obtain similar results only a 20-term correlation function is needed in the wave function compared to the 220-term wave function required in the above-mentioned calculation. Results for the phase shifts, obtained in the present hybrid formalism, are rigorous lower bounds to the exact phase shifts. The lowest P-wave resonances in He atom and hydrogen ion have also been calculated and compared with the results obtained using the Feshbach projection operator formalism [Bhatia and Temkin, Phys. Rev. A 11, 2018 (1975)] and also with the results of other calculations. It is concluded that accurate resonance parameters can be obtained by the present method, which has the advantage of including corrections due to neighboring resonances, bound states, and the continuum in which these resonances are embedded.
C1 NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bhatia, AK (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 16
TC 2
Z9 2
U1 1
U2 1
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD SEP 24
PY 2012
VL 86
IS 3
AR 032709
DI 10.1103/PhysRevA.86.032709
PG 7
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 010NS
UT WOS:000309101700009
ER
PT J
AU Grossman, L
Malin, M
AF Grossman, Lisa
Malin, Michael
TI One minute with ... Michael Malin
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [Malin, Michael] NASA, Washington, DC USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD SEP 22
PY 2012
VL 215
IS 2883
BP 25
EP 25
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 035IJ
UT WOS:000310939700015
ER
PT J
AU Boardsen, SA
Slavin, JA
Anderson, BJ
Korth, H
Schriver, D
Solomon, SC
AF Boardsen, Scott A.
Slavin, James A.
Anderson, Brian J.
Korth, Haje
Schriver, David
Solomon, Sean C.
TI Survey of coherent similar to 1 Hz waves in Mercury's inner
magnetosphere from MESSENGER observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ION-CYCLOTRON WAVES; MAGNETIC-FIELD; ULF WAVES; 1ST FLYBY; POLARIZATION;
FREQUENCY; PLASMA; PULSATIONS; RESONANCES; EXOSPHERE
AB We summarize observations by the MESSENGER spacecraft of highly coherent waves at frequencies between 0.4 and 5 Hz in Mercury's inner magnetosphere. This survey covers the time period from 24 March to 25 September 2011, or 2.1 Mercury years. These waves typically exhibit banded harmonic structure that drifts in frequency as the spacecraft traverses the magnetic equator. The waves are seen at all magnetic local times, but their observed rate of occurrence is much less on the dayside, at least in part the result of MESSENGER's orbit. On the nightside, on average, wave power is maximum near the equator and decreases with increasing magnetic latitude, consistent with an equatorial source. When the spacecraft traverses the plasma sheet during its equatorial crossings, wave power is a factor of 2 larger than for equatorial crossings that do not cross the plasma sheet. The waves are highly transverse at large magnetic latitudes but are more compressional near the equator. However, at the equator the transverse component of these waves increases relative to the compressional component as the degree of polarization decreases. Also, there is a substantial minority of events that are transverse at all magnetic latitudes, including the equator. A few of these latter events could be interpreted as ion cyclotron waves. In general, the waves tend to be strongly linear and characterized by values of the ellipticity <0.3 and wave-normal angles peaked near 90 degrees. Their maxima in wave power at the equator coupled with their narrow-band character suggests that these waves might be generated locally in loss cone plasma characterized by high values of the ratio beta of plasma pressure to magnetic pressure. Presumably both electromagnetic ion cyclotron waves and electromagnetic ion Bernstein waves can be generated by ion loss cone distributions. If proton beta decreases with increasing magnetic latitude along a field line, then electromagnetic ion Bernstein waves are predicted to transition from compressional to transverse, a pattern consistent with our observations. We hypothesize that these local instabilities can lead to enhanced ion precipitation and directly feed field-line resonances.
C1 [Boardsen, Scott A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA.
[Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Schriver, David] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA.
RP Boardsen, SA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM scott.a.boardsen@nasa.gov
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU NASA Discovery Program [NAS5-97271, NASW-00002]; NASA Planetary Data
Analysis Program [NNX10AU26G]
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to The Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington.
This work is also supported by NASA Planetary Data Analysis Program
grant NNX10AU26G.
NR 38
TC 19
Z9 19
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-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 22
PY 2012
VL 117
AR A00M05
DI 10.1029/2012JA017822
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 011AY
UT WOS:000309136900005
ER
PT J
AU Biradar, S
Goornavar, V
Periyakaruppan, A
Koehne, J
Jeffers, R
Hall, JC
Ramesh, V
Meyyappan, M
Ramesh, GT
AF Biradar, Santoshkumar
Goornavar, Virupaxi
Periyakaruppan, Adaikkappan
Koehne, Jessica
Jeffers, Robert
Hall, Joseph C.
Ramesh, Vani
Meyyappan, M.
Ramesh, Govindarajan T.
TI Optimization of process parameters of polymer solution mediated growth
of calcium carbonate nanoparticles
SO NANOTECHNOLOGY
LA English
DT Article
ID BEER-LAMBERT LAW; PP/CASO4 COMPOSITES; DELIVERY-SYSTEM; CRYSTALLIZATION;
MICROPARTICLES; ENCAPSULATION; DIFFUSION; BIOSENSOR; FILLERS; MATRIX
AB With the advent of nanotechnology, many methods of synthesis of nanoparticles have come into practice and the 'polymer mediated growth' technique is among them. In this route, ions of one of the reactants are allowed to diffuse from an external solution into a polymer matrix where the other reactant is complexed and bound. The exact role of ionic diffusion in the formation of nanoparticles was investigated in the current study by studying the patterns of kinetics of nanoparticle formation using UV vis spectroscopy. Typically, calcium carbonate nanoparticles were formed by the aforementioned technique using polyethylene glycol solution. The particle size was calculated using Scherrer's formula on x-ray diffraction plots and was reconfirmed with field emission scanning electron microscope and transmission electron microscope images. Energy-dispersive x-ray analysis was used to study the composition and purity of the nanoparticles formed. The reactant to polymer ratio, reaction temperature and molecular weight of polyethylene glycol affected the size of the particles formed. Through this knowledge we optimized these parameters to obtain particles as small as 20 nm and confirmed that this technique can be used to control the size of nanoparticles.
C1 [Biradar, Santoshkumar; Goornavar, Virupaxi; Jeffers, Robert; Hall, Joseph C.; Ramesh, Vani; Ramesh, Govindarajan T.] Norfolk State Univ, Ctr Biotechnol & Biomed Sci, Dept Biol, Mol Toxicol Lab, Norfolk, VA 23504 USA.
[Periyakaruppan, Adaikkappan; Koehne, Jessica; Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ramesh, GT (reprint author), Norfolk State Univ, Ctr Biotechnol & Biomed Sci, Dept Biol, Mol Toxicol Lab, Norfolk, VA 23504 USA.
EM gtramesh@nsu.edu
RI Periyakaruppan, Adaikkappan/B-7398-2013
OI Periyakaruppan, Adaikkappan/0000-0002-0395-6564
FU NASA NSTI; NSF-CREST
FX The authors acknowledge the help of the Center for Materials Research
and Center for Biotechnology and Biomedical Sciences, Norfolk State
University, Norfolk, VA for their resources, in particular Dr A K
Pradhan, for his help in the use of XRD equipment. The authors also
acknowledge the help of the Jefferson Laboratory, Newport News, VA for
FESEM/EDX analysis and the NASA AMES Research Center, San Francisco, CA
for TEM images. This work was supported by NASA NSTI and NSF-CREST.
NR 27
TC 1
Z9 1
U1 2
U2 30
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD SEP 21
PY 2012
VL 23
IS 37
AR 375601
DI 10.1088/0957-4484/23/37/375601
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 006HT
UT WOS:000308810800010
PM 22922538
ER
PT J
AU Nobili, AM
Shao, M
Pegna, R
Zavattini, G
Turyshev, SG
Lucchesi, DM
De Michele, A
Doravari, S
Comandi, GL
Saravanan, TR
Palmonari, F
Catastini, G
Anselmi, A
AF Nobili, A. M.
Shao, M.
Pegna, R.
Zavattini, G.
Turyshev, S. G.
Lucchesi, D. M.
De Michele, A.
Doravari, S.
Comandi, G. L.
Saravanan, T. R.
Palmonari, F.
Catastini, G.
Anselmi, A.
TI 'Galileo Galilei' (GG): space test of the weak equivalence principle to
10(-17) and laboratory demonstrations
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID MISSION; ENERGY
AB The small satellite 'Galileo Galilei' (GG) will test the universality of free fall and hence the weak equivalence principle which is the founding pillar of general relativity to 1 part in 10(17). It will use proof masses whose atoms differ substantially from one another in their mass energy content, so as to maximize the chance of violation. GG will improve by four orders of magnitude the current best 'Eot-Wash' tests based on slowly rotating torsion balances, which have been able to reach their thermal noise level. In GG, the expected violation signal is a relative displacement between the proof masses of similar or equal to 0.6 pm caused by a differential acceleration alpha(GG) similar or equal to 8 x 10(-17) ms(-2) pointing to the center of mass of the Earth as the satellite orbits around it at nu(GG) similar or equal to 1.7 x 10(-4) Hz. GG will fly an innovative acceleration sensor based on rapidly rotating macroscopic test masses weakly coupled in 2D which up-converts the signal to nu(spin) similar or equal to 1 Hz, a value well above the frequency of natural oscillations of the masses relative to each other nu(d) = 1/T-d similar or equal to 1/(540 s). The sensor is unique in that it ensures high rotation frequency, low thermal noise and no attenuation of the signal strength (Pegna et al 2011 Phys. Rev. Lett. 107 200801). A readout based on a very low noise laser interferometry gauge developed at Jet Propulsion Laboratory (similar or equal to 1 pm Hz(-1/2) at 1 Hz demonstrated) allows the short integration time to be fully exploited. A full scale sensor with the same degrees of freedom and the same dynamical features as the one to fly in GG has been setup on ground (GGG). The proof masses of GGG are affected by acceleration and tilt noise acting on the rotating shaft because of ball bearings and terrain microseismicity (both absent in space). Overall, by means of appropriate 2D flexure joints, these noise sources have been reduced by a factor almost 10(5) down to a differential acceleration between the proof masses of similar or equal to 7 x 10(-11) m s(-2) (at 1.7 x 10(-4) Hz up-converted by rotation to similar or equal to 0.2Hz). The corresponding noise in the relative displacements of the proof masses, read by co-rotating capacitance bridges, is similar or equal to 180 pm, which is 300 times larger than the target in space. GGG error budget shows that it can reach a differential acceleration sensitivity alpha(GGGgoal) similar or equal to 8 x 10(-16) m s(-2), not limited by thermal noise. This value is only a factor 10 larger than what GG must reach in space to meet its target, and slightly smaller than the acceleration noise of the torsion balance. It can be achieved partly by means of weaker joints and an optimized mechanical design-so as to improve the attenuation factor-and partly by replacing the current ball bearings with much less noisy air bearings (also used in torsion balance tests) so as to reduce input noise. A laser gauge readout with noise level r(laser-ro) similar or equal to 30 pm Hz(-1/2) at 0.2 divided by 3 Hz will be implemented.
C1 [Nobili, A. M.; De Michele, A.; Saravanan, T. R.] Univ Pisa, Dept Phys E Fermi, I-56127 Pisa, Italy.
[Nobili, A. M.; Pegna, R.; Lucchesi, D. M.; Comandi, G. L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Shao, M.; Turyshev, S. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zavattini, G.] Univ Ferrara, Dept Phys, I-44122 Ferrara, Italy.
[Zavattini, G.] Ist Nazl Fis Nucl, Sez Ferrara, I-44122 Ferrara, Italy.
[Doravari, S.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Palmonari, F.] Univ Bologna, Dept Phys, I-40127 Bologna, Italy.
[Palmonari, F.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Catastini, G.; Anselmi, A.] Thales Alenia Space Italia, I-10146 Turin, Italy.
[Lucchesi, D. M.] IAPS, INAF, I-00133 Rome, Italy.
RP Nobili, AM (reprint author), Univ Pisa, Dept Phys E Fermi, Largo Bruno Pontecorvo 3, I-56127 Pisa, Italy.
EM nobili@dm.unipi.it
FU ASI; INFN; NASA
FX This work was supported by ASI and INFN and it was performed in part at
JPL, Caltech, under a contract with NASA. The authors also thank the
referees whose thorough analysis has helped in making the paper much
better than it was when submitted.
NR 48
TC 23
Z9 23
U1 0
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD SEP 21
PY 2012
VL 29
IS 18
AR 184011
DI 10.1088/0264-9381/29/18/184011
PG 18
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 993RO
UT WOS:000307877500012
ER
PT J
AU Williams, JG
Turyshev, SG
Boggs, DH
AF Williams, James G.
Turyshev, Slava G.
Boggs, Dale H.
TI Lunar laser ranging tests of the equivalence principle
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID GENERAL-RELATIVITY; MOON; GRAVITY; PHYSICS; APOLLO; EARTH
AB The lunar laser ranging (LLR) experiment provides precise observations of the lunar orbit that contribute to a wide range of science investigations. In particular, time series of highly accurate measurements of the distance between the Earth and Moon provide unique information that determine whether, in accordance with the equivalence principle (EP), both of these celestial bodies are accelerating toward the Sun at the same rate, despite their different masses, compositions, and gravitational self-energies. Analyses of precise laser ranges to the Moon continue to provide increasingly stringent limits on any violation of the EP. Current LLR solutions give (-0.8 +/- 1.3) x 10(-13) for any possible inequality in the ratios of the gravitational and inertial masses for the Earth and Moon, (mG/mI)E - (mG/mI) M. Such an accurate result allows other tests of gravitational theories. Focusing on the tests of the EP, we discuss the existing data and data analysis techniques. The robustness of the LLR solutions is demonstrated with several different approaches to solutions. Additional high accuracy ranges and improvements in the LLR data analysis model will further advance the research of relativistic gravity in the solar system, and will continue to provide highly accurate tests of the EP.
C1 [Williams, James G.; Turyshev, Slava G.; Boggs, Dale H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Williams, JG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM james.g.williams@jpl.nasa.gov; turyshev@jpl.nasa.gov;
dale.h.boggs@jpl.nasa.gov
NR 31
TC 44
Z9 46
U1 1
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD SEP 21
PY 2012
VL 29
IS 18
AR 184004
DI 10.1088/0264-9381/29/18/184004
PG 11
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 993RO
UT WOS:000307877500005
ER
PT J
AU Rychert, CA
Schmerr, N
Harmon, N
AF Rychert, Catherine A.
Schmerr, Nicholas
Harmon, Nicholas
TI The Pacific lithosphere-asthenosphere boundary: Seismic imaging and
anisotropic constraints from SS waveforms
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE Pacific; anisotropy; body waves; lithosphere-asthenosphere; oceanic
lithosphere; seismic
ID UPPER-MANTLE STRUCTURE; OCEANIC UPPER-MANTLE; STRUCTURE BENEATH; 520-KM
DISCONTINUITY; HAWAIIAN PLUME; LOW-VELOCITY; HEAT-FLOW; ZONE; MELT;
TOMOGRAPHY
AB The lithosphere-asthenosphere boundary (LAB) separating the rigid lid from the underlying weaker, convecting asthenosphere is a fundamental interface in mantle dynamics and plate tectonics. However, the exact depth and defining mechanism of the LAB interface remain poorly understood. The ocean plates are ideal for testing hypotheses regarding the nature of a plate since they make up 70% of Earth's surface area and have a relatively simple geological history. Seismically imaging the oceanic LAB at high resolution has proved challenging. Yet, several studies have recently increased resolution with provocative results. We summarize recent imaging of discontinuity structure beneath much of the Pacific using receiver functions from ocean floor borehole seismometers and land stations located at ocean-continent margins, SS precursors, and waveform modeling of multiple phases including multiple bounce S waves, ScS reverberations, and surface waves. Overall, there is much agreement among these different approaches about the reported depth of a negative discontinuity that occurs near the expected depth of the LAB. Some of the apparent discrepancies in depth are explained by the variation in sensitivity of seismic waves that sample structure at different wavelengths. Yet, when the results are considered together, no single age-depth relationship is illuminated. There are also puzzling discrepancies in where the discontinuity is detected, which again suggests greater complexity. Here we test the possibility that discrepant detection of a strong sharp discontinuity is caused by anisotropic structure. We stack SS waveforms with bounce points in the central Pacific into azimuthal bins. We use two methods, one that inverts for discontinuity structure based on subtle variations in the character of the SS waveform, and another that considers SS at higher frequency. We find azimuthal variation in the amplitude of the waveform, including a polarity reversal. We suggest that anisotropy is an important factor in imaging and constraining discontinuity structure of the oceanic plate, and must be carefully considered to constrain the age-depth dependence and defining mechanism of the oceanic lithosphere.
C1 [Rychert, Catherine A.; Harmon, Nicholas] Univ Southampton, Natl Oceanog Ctr Southampton, Southampton SO14 3ZH, Hants, England.
[Schmerr, Nicholas] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Rychert, CA (reprint author), Univ Southampton, Natl Oceanog Ctr Southampton, Southampton SO14 3ZH, Hants, England.
EM c.rychert@soton.ac.uk
OI Schmerr, Nicholas/0000-0002-3256-1262
FU Natural Environment Research Council - UK [NE/G013438/1]; NASA
FX We thank Hitoshi Kawakatsu for helpful comments on an earlier version of
the manuscript and Prakash Kumar for providing his receiver function
results and locations. We thank Meredith Nettles for providing her
surface wave velocity model. We acknowledge funding from the Natural
Environment Research Council - UK (NE/G013438/1) [CAR] and NASA
postdoctoral program [NS]. Data are obtained from the IRIS Data
Management Center. Figures made using GMT.
NR 85
TC 14
Z9 14
U1 1
U2 35
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD SEP 21
PY 2012
VL 13
AR Q0AK10
DI 10.1029/2012GC004194
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 011AG
UT WOS:000309135100001
ER
PT J
AU Kuang, S
Newchurch, MJ
Burris, J
Wang, LH
Knupp, K
Huang, GY
AF Kuang, Shi
Newchurch, M. J.
Burris, John
Wang, Lihua
Knupp, Kevin
Huang, Guanyu
TI Stratosphere-to-troposphere transport revealed by ground-based lidar and
ozonesonde at a midlatitude site
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CROSS-TROPOPAUSE EXCHANGE; POTENTIAL VORTICITY; CUTOFF LOW; DYNAMICAL
TROPOPAUSE; NORTHERN-HEMISPHERE; EXTRATROPICAL TROPOPAUSE; GLOBAL
TROPOPAUSE; BOUNDARY-LAYER; UNITED-STATES; CLOUD LIQUID
AB This paper presents ozone structures measured by a ground-based ozone lidar and ozonesonde at Huntsville, Alabama, on 27-29 April 2010 originating from a stratosphere-to-troposphere transport event associated with a cutoff cyclone and tropopause fold. In this case, the tropopause reached 6 km and the stratospheric intrusion resulted in a 2-km thick elevated ozone layer with values between 70 and 85 ppbv descending from the similar to 306-K to 298-K isentropic surface at a rate of similar to 5 km day(-1). The potential temperature was provided by a collocated microwave profiling radiometer. We examine the corresponding meteorological fields and potential vorticity (PV) structures derived from the analysis data from the North American Mesoscale model. The 2-PVU (PV unit) surface, defined as the dynamic tropopause, is able to capture the variations of the ozone tropopause estimated from the ozonesonde and lidar measurements. The estimated ozone/PV ratio, from the measured ozone and model derived PV, for the mixing layer between the troposphere and stratosphere is similar to 41 ppbv/PVU with an uncertainty of similar to 33%. Within two days, the estimated mass of ozone irreversibly transported from the stratospheric into the troposphere is between 0.07 Tg (0.9 x 10(33) molecules) and 0.11 Tg (1.3 x 10(33) molecules) with an estimated uncertainty of 59%. Tropospheric ozone exhibited enormous variability due to the complicated mixing processes. Low ozone and large variability were observed in the mid-troposphere after the stratospheric intrusion due to the westerly advection including the transition from a cyclonic system to an anticyclonic system. This study using high temporal and vertical-resolution measurements suggests that, in this case, stratospheric air quickly lost its stratospheric characteristics once it is irreversibly mixed down into the troposphere.
C1 [Kuang, Shi; Newchurch, M. J.; Wang, Lihua; Knupp, Kevin; Huang, Guanyu] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA.
[Burris, John] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kuang, S (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM kuang@nsstc.uah.edu
OI Huang, Guanyu/0000-0001-7314-8485; Kuang, Shi/0000-0003-2423-6088
FU NASA's Science Mission Directorate; NOAA's National Environmental
Satellite, Data, and Information Service (NESDIS)
FX The authors would like to thank Tom McGee of NASA/GSFC, Stuart McDermid
and Thierry Leblanc of NASA/JPL for extensive discussions about lidar
instrumentation, Wesley Cantrell of UAHuntsville for providing the
ozonesonde data, and the NASA/GSFC OMI working group for providing the
OMI column ozone data. This work was supported by NASA's Science Mission
Directorate and NOAA's National Environmental Satellite, Data, and
Information Service (NESDIS). The UAHuntsville RAPCD ozone lidar is
affiliated with the Network for Detection of Atmospheric Composition
Change (NDACC), and its data are publicly available at
http://www.ndacc.org and http://nsstc.uah.edu/atmchem.
NR 81
TC 18
Z9 20
U1 2
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 21
PY 2012
VL 117
AR D18305
DI 10.1029/2012JD017695
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 011BU
UT WOS:000309139200005
ER
PT J
AU Leinonen, J
Kneifel, S
Moisseev, D
Tyynela, J
Tanelli, S
Nousiainen, T
AF Leinonen, J.
Kneifel, S.
Moisseev, D.
Tyynela, J.
Tanelli, S.
Nousiainen, T.
TI Evidence of nonspheroidal behavior in millimeter-wavelength radar
observations of snowfall
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PRECIPITATION RADAR; ICE PARTICLES; SCATTERING; BACKSCATTERING; SURFACE;
SNOWFLAKES; RETRIEVAL; WATER
AB Recent modeling results have indicated that, in general, idealized homogeneous spheroidal models of ice crystals and snowflakes cannot consistently describe radar backscattering from snowfall when the radar wavelengths are on the order of the snowflake size. In this paper, we provide empirical evidence supporting this prediction by analyzing collocated airborne radar measurements at 13.4 GHz, 35.6 GHz and 94 GHz. The analysis is performed by applying a recently developed method making use of two simultaneously measured dualq-frequency ratios, allowing one to distinguish between the multifrequency backscattering behavior of detailed aggregate snow models and that of homogeneous spheroids. We demonstrate that in some naturally occurring cases, detailed snowflake models, which account for their complex structure, are required to describe backscattering by these particles in a manner that is consistent over multiple wavelengths. This implies that the spheroidal approximation is not always adequate as a snowflake shape model in radar retrievals at this wavelength range.
C1 [Leinonen, J.] Finnish Meteorol Inst, FI-00101 Helsinki, Finland.
[Leinonen, J.] Aalto Univ, Dept Appl Phys, Espoo, Finland.
[Kneifel, S.] Univ Cologne, Inst Geophys & Meteorol, D-50931 Cologne, Germany.
[Moisseev, D.; Tyynela, J.; Nousiainen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Leinonen, J (reprint author), Finnish Meteorol Inst, FI-00101 Helsinki, Finland.
EM jussi.leinonen@fmi.fi
RI Nousiainen, Timo/A-7982-2008; Moisseev, Dmitri/A-3288-2008; Kneifel,
Stefan/A-2044-2015;
OI Nousiainen, Timo/0000-0002-6569-9815; Moisseev,
Dmitri/0000-0002-4575-0409; Kneifel, Stefan/0000-0003-2220-2968;
Leinonen, Jussi/0000-0002-6560-6316
FU Academy of Finland [125180, 128255, 128328]; National Aeronautics and
Space Administration
FX This work was supported by grants 125180, 128255 and 128328 from the
Academy of Finland. We thank Grant Petty for providing the results for
his aggregate calculations. The contributions by S. Tanelli were
performed at the Jet Propulsion Laboratory under contract with the
National Aeronautics and Space Administration; support from R. Kakar and
H. Maring at NASA HQ is gratefully acknowledged.
NR 41
TC 21
Z9 22
U1 2
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 21
PY 2012
VL 117
AR D18205
DI 10.1029/2012JD017680
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 011BU
UT WOS:000309139200004
ER
PT J
AU Ryder, I
Burgmann, R
Fielding, E
AF Ryder, Isabelle
Buergmann, Roland
Fielding, Eric
TI Static stress interactions in extensional earthquake sequences: An
example from the South Lunggar Rift, Tibet
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID FAULT SYSTEMS
AB An extensional earthquake sequence occurred in 2004-8 across a graben in the South Lunggar Rift on the Tibetan Plateau. We use InSAR data to determine the location, fault geometry and slip distribution of these earthquakes and to test whether the sequence is compatible with static stress triggering. The Mw 6.2 and 6.3 earthquakes in 2004 and 2005 both ruptured west-dipping faults on the east side of a graben. In 2008, a Mw 6.7 earthquake ruptured a pair of east-dipping fault segments on the other side of the graben, offset from the earlier ruptures. We compute first-order dislocation models of stress change and demonstrate that the order and spatial configuration of this sequence of events is compatible with triggering by static stress transfer. A continuation of the sequence would be most likely to occur on the northern extension of the 2008 rupture, although variable slip rate along the rift may mean that the sequence has run its course. The InSAR data for the 2008 earthquake also reveal slip on a fault that cuts the graben at a highly oblique angle. We suggest that this is a release fault accommodating differential throw in the hanging wall, and associate the deformation with a Mw 6.0 aftershock. Activity on such a release fault has not been directly imaged before. The Zhongba sequence is one of several examples of recent clustered normal-fault earthquakes on the Plateau, and may be an example of phase-locking of similar faults.
C1 [Ryder, Isabelle] Univ Liverpool, Sch Environm Sci, Liverpool L69 3GP, Merseyside, England.
[Buergmann, Roland] Univ Calif Berkeley, Berkeley Seismol Lab, Berkeley, CA 94720 USA.
[Fielding, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Ryder, I (reprint author), Univ Liverpool, Sch Environm Sci, Liverpool L69 3GP, Merseyside, England.
EM i.ryder@liv.ac.uk
RI Fielding, Eric/A-1288-2007
OI Fielding, Eric/0000-0002-6648-8067
FU NSF [EAR-1014880]; ESA Category-1 award [C1P.5119, ESA AO 668]; NASA
Earth Science and Interior Focus Area
FX This research was started as part of NSF grant EAR-1014880. Envisat data
are copyright ESA and were obtained through ESA Category-1 award
C1P.5119 and ESA AO 668. Part of this research was sponsored by the NASA
Earth Science and Interior Focus Area and performed at the Jet
Propulsion Laboratory, California Institute of Technology, Pasadena,
California. Several figures in this paper were produced using the
Coulomb software (version 3.2.01), and Figure 1a was produced using
GeoMapApp (version 3.1.6).
NR 24
TC 7
Z9 7
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD SEP 21
PY 2012
VL 117
AR B09405
DI 10.1029/2012JB009365
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 011AR
UT WOS:000309136200001
ER
PT J
AU Orosz, JA
Welsh, WF
Carter, JA
Fabrycky, DC
Cochran, WD
Endl, M
Ford, EB
Haghighipour, N
MacQueen, PJ
Mazeh, T
Sanchis-Ojeda, R
Short, DR
Torres, G
Agol, E
Buchhave, LA
Doyle, LR
Isaacson, H
Lissauer, JJ
Marcy, GW
Shporer, A
Windmiller, G
Barclay, T
Boss, AP
Clarke, BD
Fortney, J
Geary, JC
Holman, MJ
Huber, D
Jenkins, JM
Kinemuchi, K
Kruse, E
Ragozzine, D
Sasselov, D
Still, M
Tenenbaum, P
Uddin, K
Winn, JN
Koch, DG
Borucki, WJ
AF Orosz, Jerome A.
Welsh, William F.
Carter, Joshua A.
Fabrycky, Daniel C.
Cochran, William D.
Endl, Michael
Ford, Eric B.
Haghighipour, Nader
MacQueen, Phillip J.
Mazeh, Tsevi
Sanchis-Ojeda, Roberto
Short, Donald R.
Torres, Guillermo
Agol, Eric
Buchhave, Lars A.
Doyle, Laurance R.
Isaacson, Howard
Lissauer, Jack J.
Marcy, Geoffrey W.
Shporer, Avi
Windmiller, Gur
Barclay, Thomas
Boss, Alan P.
Clarke, Bruce D.
Fortney, Jonathan
Geary, John C.
Holman, Matthew J.
Huber, Daniel
Jenkins, Jon M.
Kinemuchi, Karen
Kruse, Ethan
Ragozzine, Darin
Sasselov, Dimitar
Still, Martin
Tenenbaum, Peter
Uddin, Kamal
Winn, Joshua N.
Koch, David G.
Borucki, William J.
TI Kepler-47: A Transiting Circumbinary Multiplanet System
SO SCIENCE
LA English
DT Article
ID SPIN-ORBIT ALIGNMENT; HIERARCHICAL TRIPLE; PLANETS; STARSPOTS
AB We report the detection of Kepler-47, a system consisting of two planets orbiting around an eclipsing pair of stars. The inner and outer planets have radii 3.0 and 4.6 times that of Earth, respectively. The binary star consists of a Sun-like star and a companion roughly one-third its size, orbiting each other every 7.45 days. With an orbital period of 49.5 days, 18 transits of the inner planet have been observed, allowing a detailed characterization of its orbit and those of the stars. The outer planet's orbital period is 303.2 days, and although the planet is not Earth-like, it resides within the classical "habitable zone," where liquid water could exist on an Earth-like planet. With its two known planets, Kepler-47 establishes that close binary stars can host complete planetary systems.
C1 [Orosz, Jerome A.; Welsh, William F.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Carter, Joshua A.; Torres, Guillermo; Geary, John C.; Holman, Matthew J.; Kruse, Ethan; Ragozzine, Darin; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel C.; Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
[Doyle, Laurance R.; Clarke, Bruce D.; Jenkins, Jon M.; Tenenbaum, Peter] SETI Inst, Mountain View, CA 94043 USA.
[Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Lissauer, Jack J.; Barclay, Thomas; Clarke, Bruce D.; Huber, Daniel; Jenkins, Jon M.; Kinemuchi, Karen; Still, Martin; Tenenbaum, Peter; Uddin, Kamal; Koch, David G.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Shporer, Avi] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA.
[Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Barclay, Thomas; Kinemuchi, Karen] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
[Boss, Alan P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Uddin, Kamal] Orbital Sci Corp, Dulles, VA 20166 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA.
EM orosz@sciences.sdsu.edu
RI Carter, Joshua/A-8280-2013; Sanchis-Ojeda, Roberto/B-6574-2013; Agol,
Eric/B-8775-2013; Ragozzine, Darin/C-4926-2013;
OI Sanchis-Ojeda, Roberto/0000-0002-6193-972X; Agol,
Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354; Kruse,
Ethan/0000-0002-0493-1342; Buchhave, Lars A./0000-0003-1605-5666;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA, Science Mission Directorate; NASA [NAS5-26555, NNX12AD23G,
HF-51267.01-A, HF-51272.01-A]; NASA Office of Space Science
[NXX09AF08G]; NSF [AST-1109928, AST-1007992]; STScI
FX Kepler was selected as the 10th mission of the Discovery Program.
Funding for this mission is provided by NASA, Science Mission
Directorate. The Kepler data presented in this paper were obtained from
the Mikulski Archive for Space Telescopes (MAST). The Space Telescope
Science Institute (STScI) is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support
for MAST for non-HTS data is provided by the NASA Office of Space
Science via grant NXX09AF08G and by other grants and contracts. This
work is based in part on observations obtained with the Hobby-Eberly
Telescope, which is a joint project of the University of Texas at
Austin, the Pennsylvania State University, Stanford University,
Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat
Gottingen. J.A.O. and W.F.W. acknowledge support from the Kepler
Participating Scientist Program via NASA grant NNX12AD23G; J.A.O.,
W.F.W., and G.W. also gratefully acknowledge support from the NSF via
grant AST-1109928. G.T. acknowledges partial support for this work from
NSF grant AST-1007992. J.A.C. and D.C.F. acknowledge NASA support
through Hubble Fellowship grants HF-51267.01-A and HF-51272.01-A,
respectively, awarded by STScI. Our dear friend and colleague David G.
Koch passed away after this work was completed. He was a critical part
of Kepler's success, and he will be missed.
NR 21
TC 137
Z9 139
U1 2
U2 12
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD SEP 21
PY 2012
VL 337
IS 6101
BP 1511
EP 1514
DI 10.1126/science.1228380
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 007UC
UT WOS:000308912900044
PM 22933522
ER
PT J
AU Zheng, W
Postman, M
Zitrin, A
Moustakas, J
Shu, XW
Jouvel, S
Host, O
Molino, A
Bradley, L
Coe, D
Moustakas, LA
Carrasco, M
Ford, H
Benitez, N
Lauer, TR
Seitz, S
Bouwens, R
Koekemoer, A
Medezinski, E
Bartelmann, M
Broadhurst, T
Donahue, M
Grillo, C
Infante, L
Jha, SW
Kelson, DD
Lahav, O
Lemze, D
Melchior, P
Meneghetti, M
Merten, J
Nonino, M
Ogaz, S
Rosati, P
Umetsu, K
van der Wel, A
AF Zheng, Wei
Postman, Marc
Zitrin, Adi
Moustakas, John
Shu, Xinwen
Jouvel, Stephanie
Host, Ole
Molino, Alberto
Bradley, Larry
Coe, Dan
Moustakas, Leonidas A.
Carrasco, Mauricio
Ford, Holland
Benitez, Narciso
Lauer, Tod R.
Seitz, Stella
Bouwens, Rychard
Koekemoer, Anton
Medezinski, Elinor
Bartelmann, Matthias
Broadhurst, Tom
Donahue, Megan
Grillo, Claudio
Infante, Leopoldo
Jha, Saurabh W.
Kelson, Daniel D.
Lahav, Ofer
Lemze, Doron
Melchior, Peter
Meneghetti, Massimo
Merten, Julian
Nonino, Mario
Ogaz, Sara
Rosati, Piero
Umetsu, Keiichi
van der Wel, Arjen
TI A magnified young galaxy from about 500 million years after the Big Bang
SO NATURE
LA English
DT Article
ID SIMILAR-TO 7; STELLAR POPULATION SYNTHESIS; DEEP SURVEY; CLUSTER;
BRIGHT; DISCOVERY; HUBBLE; MACS; REIONIZATION; CALIBRATION
AB Re-ionization of the intergalactic medium occurred in the early Universe at redshift z approximate to 6-11, following the formation of the first generation of stars(1). Those young galaxies (where the bulk of stars formed) at a cosmic age of less than about 500 million years (z less than or similar to 10) remain largely unexplored because they are at or beyond the sensitivity limits of existing large telescopes. Understanding the properties of these galaxies is critical to identifying the source of the radiation that re-ionized the intergalactic medium. Gravitational lensing by galaxy clusters allows the detection of high-redshift galaxies fainter than what otherwise could be found in the deepest images of the sky(2). Here we report multiband observations of the cluster MACS J1149+2223 that have revealed (with high probability) a gravitationally magnified galaxy from the early Universe, at a redshift of z = 9.6 +/- 0.2 (that is, a cosmic age of 490 +/- 15 million years, or 3.6 per cent of the age of the Universe). We estimate that it formed less than 200 million years after the Big Bang (at the 95 per cent confidence level), implying a formation redshift of less than or similar to 14. Given the small sky area that our observations cover, faint galaxies seem to be abundant at such a young cosmic age, suggesting that they may be the dominant source for the early re-ionization of the intergalactic medium.
C1 [Zheng, Wei; Ford, Holland; Medezinski, Elinor; Lemze, Doron] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Postman, Marc; Bradley, Larry; Coe, Dan; Koekemoer, Anton; Ogaz, Sara] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Zitrin, Adi; Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
[Shu, Xinwen] Univ Sci & Technol China, Dept Astron, Hefei 230026, Anhui, Peoples R China.
[Jouvel, Stephanie; Host, Ole; Lahav, Ofer] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Jouvel, Stephanie] Inst Ciencies Espai, Bellaterra 08193, Spain.
[Molino, Alberto; Benitez, Narciso] Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Moustakas, Leonidas A.; Merten, Julian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Carrasco, Mauricio; Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Lauer, Tod R.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Seitz, Stella] Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Bouwens, Rychard] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Broadhurst, Tom] Univ Basque Country, Dept Theoret Phys, Bilbao 48080, Spain.
[Broadhurst, Tom] Basque Fdn Sci, Ikerbasque, Bilbao 48011, Spain.
[Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Grillo, Claudio] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Kelson, Daniel D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Nonino, Mario] INAF Osservatorio Astron Trieste, I-40131 Trieste, Italy.
[Meneghetti, Massimo] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Rosati, Piero] European So Observ, D-85748 Garching, Germany.
[Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Zheng, W (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM zheng@pha.jhu.edu
RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014;
Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; Shu,
Xinwen/D-7294-2017;
OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti,
Massimo/0000-0003-1225-7084; Shu, Xinwen/0000-0002-7020-4290; Nonino,
Mario/0000-0001-6342-9662; Koekemoer, Anton/0000-0002-6610-2048; Umetsu,
Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360;
Benitez, Narciso/0000-0002-0403-7455
FU NASA [NAS 5-26555]; NSF [AST-0908246]; Baden Wurttemberg Stiftung
FX The CLASH programme (GO-12065) is based on observations made with the
NASA/ESA Hubble Space Telescope. The Space Telescope Science Institute
is operated by the Association of Universities for Research in
Astronomy, Inc. under NASA contract NAS 5-26555. This work is also based
in part on archival data obtained with the Spitzer Space Telescope,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology under a contract with NASA. J.M. acknowledges support from
NSF grant AST-0908246. A. Z. is supported by research contract
Internationale Spitzenforschung II-1 of the Baden Wurttemberg Stiftung.
NR 30
TC 139
Z9 139
U1 9
U2 39
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD SEP 20
PY 2012
VL 489
IS 7416
BP 406
EP 408
DI 10.1038/nature11446
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 007AK
UT WOS:000308860900039
PM 22996554
ER
PT J
AU Aguirre, VS
Casagrande, L
Basu, S
Campante, TL
Chaplin, WJ
Huber, D
Miglio, A
Serenelli, AM
Ballot, J
Bedding, TR
Christensen-Dalsgaard, J
Creevey, OL
Elsworth, Y
Garcia, RA
Gilliland, RL
Hekker, S
Kjeldsen, H
Mathur, S
Metcalfe, TS
Monteiro, MJPFG
Mosser, B
Pinsonneault, MH
Stello, D
Weiss, A
Tenenbaum, P
Twicken, JD
Uddin, K
AF Aguirre, V. Silva
Casagrande, L.
Basu, S.
Campante, T. L.
Chaplin, W. J.
Huber, D.
Miglio, A.
Serenelli, A. M.
Ballot, J.
Bedding, T. R.
Christensen-Dalsgaard, J.
Creevey, O. L.
Elsworth, Y.
Garcia, R. A.
Gilliland, R. L.
Hekker, S.
Kjeldsen, H.
Mathur, S.
Metcalfe, T. S.
Monteiro, M. J. P. F. G.
Mosser, B.
Pinsonneault, M. H.
Stello, D.
Weiss, A.
Tenenbaum, P.
Twicken, J. D.
Uddin, K.
TI VERIFYING ASTEROSEISMICALLY DETERMINED PARAMETERS OF KEPLER STARS USING
HIPPARCOS PARALLAXES: SELF-CONSISTENT STELLAR PROPERTIES AND DISTANCES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE asteroseismology; parallaxes; stars: distances; stars: fundamental
parameters; stars: oscillations
ID SOLAR-LIKE OSCILLATIONS; GENEVA-COPENHAGEN SURVEY; INFRARED FLUX METHOD;
MAIN-SEQUENCE STARS; GIANT BRANCH STARS; RED GIANTS; EFFECTIVE
TEMPERATURES; CHEMICAL EVOLUTION; ANGULAR DIAMETERS; HELIUM ABUNDANCE
AB Accurately determining the properties of stars is of prime importance for characterizing stellar populations in our Galaxy. The field of asteroseismology has been thought to be particularly successful in such an endeavor for stars in different evolutionary stages. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of the results is mandatory. With this purpose, we present a new technique to obtain stellar properties by coupling asteroseismic analysis with the InfraRed Flux Method. By using two global seismic observables and multi-band photometry, the technique allows us to obtain masses, radii, effective temperatures, bolometric fluxes, and hence distances for field stars in a self-consistent manner. We apply our method to 22 solar-like oscillators in the Kepler short-cadence sample, that have accurate Hipparcos parallaxes. Our distance determinations agree to better than 5%, while measurements of spectroscopic effective temperatures and interferometric radii also validate our results. We briefly discuss the potential of our technique for stellar population analysis and models of Galactic Chemical Evolution.
C1 [Aguirre, V. Silva; Chaplin, W. J.; Bedding, T. R.; Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Aguirre, V. Silva; Weiss, A.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Aguirre, V. Silva; Chaplin, W. J.; Serenelli, A. M.; Christensen-Dalsgaard, J.; Garcia, R. A.; Mathur, S.; Pinsonneault, M. H.] Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Casagrande, L.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Campante, T. L.; Monteiro, M. J. P. F. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Campante, T. L.; Monteiro, M. J. P. F. G.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
[Campante, T. L.; Miglio, A.; Elsworth, Y.; Hekker, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Serenelli, A. M.] Fac Ciencies, Inst Ciencias Espacio CSIC IEEC, E-08193 Bellaterra, Spain.
[Ballot, J.] Inst Rech Astrophys & Planetol, CNRS, F-31400 Toulouse, France.
[Ballot, J.] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
[Bedding, T. R.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Creevey, O. L.] Univ Nice Sophia Antipolis, Lab Lagrange, Observ Cote Azur, CNRS,UMR 7293, F-06304 Nice 4, France.
[Garcia, R. A.] Univ Paris Diderot, Lab AIM, Ctr Saclay, CEA,DSM,CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France.
[Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA.
[Mosser, B.] Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Pinsonneault, M. H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Tenenbaum, P.; Twicken, J. D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Uddin, K.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Aguirre, VS (reprint author), Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
RI Ballot, Jerome/G-1019-2010; Weiss, Achim/C-4870-2013; Monteiro, Mario
J.P.F.G./B-4715-2008;
OI Weiss, Achim/0000-0002-3843-1653; Monteiro, Mario
J.P.F.G./0000-0003-0513-8116; Bedding, Timothy/0000-0001-5943-1460;
Metcalfe, Travis/0000-0003-4034-0416; Bedding, Tim/0000-0001-5222-4661;
Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776;
Serenelli, Aldo/0000-0001-6359-2769
FU NASA's Science Mission Directorate; National Science Foundation of the
United States [NSF PHY0551164]; Excellence cluster "Origin and Structure
of the Universe" (Garching); The Danish National Research Foundation;
European Research Council [267864]; NSF [AST-1105930]; FCT/MCTES,
Portugal [PTDC/CTE-AST/098754/2008]; UK Science Technology and
Facilities Council (STFC); NASA; European Union [PIRG-GA-2009-247732];
MICINN [AYA2011-24704]; Netherlands Organisation for Scientific Research
(NWO); Australian Research Council
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors thank the entire Kepler team, without whom
these results would not be possible. We also thank all of the funding
councils and agencies that have supported the activities of KASC Working
Group 1. We are also grateful for support from the International Space
Science Institute (ISSI). The authors acknowledge the KITP staff of UCSB
for their warm hospitality during the research program "Asteroseismology
in the Space Age." This KITP program was supported in part by the
National Science Foundation of the United States under grant No. NSF
PHY0551164. V.S.A. received financial support from the Excellence
cluster "Origin and Structure of the Universe" (Garching). Funding for
the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation. The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (Grant agreement No. 267864). S.B.
acknowledges the NSF grant AST-1105930. T.L.C. and M.J.P.F.G.M.
acknowledge financial support from project PTDC/CTE-AST/098754/2008
funded by FCT/MCTES, Portugal. W.J.C. and Y.E. acknowledge the financial
support of the UK Science Technology and Facilities Council (STFC). D.H.
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. A.M.S. is partially supported by the
European Union International Reintegration Grant PIRG-GA-2009-247732 and
the MICINN grant AYA2011-24704. S.H. acknowledges financial support from
the Netherlands Organisation for Scientific Research (NWO). D.S.
acknowledges support from the Australian Research Council. NCAR is
partially funded by the National Science Foundation.
NR 98
TC 71
Z9 71
U1 2
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 99
DI 10.1088/0004-637X/757/1/99
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800099
ER
PT J
AU Coe, D
Umetsu, K
Zitrin, A
Donahue, M
Medezinski, E
Postman, M
Carrasco, M
Anguita, T
Geller, MJ
Rines, KJ
Diaferio, A
Kurtz, MJ
Bradley, L
Koekemoer, A
Zheng, W
Nonino, M
Molino, A
Mahdavi, A
Lemze, D
Infante, L
Ogaz, S
Melchior, P
Host, O
Ford, H
Grillo, C
Rosati, P
Jimenez-Teja, Y
Moustakas, J
Broadhurst, T
Ascaso, B
Lahav, O
Bartelmann, M
Benitez, N
Bouwens, R
Graur, O
Graves, G
Jha, S
Jouvel, S
Kelson, D
Moustakas, L
Maoz, D
Meneghetti, M
Merten, J
Riess, A
Rodney, S
Seitz, S
AF Coe, Dan
Umetsu, Keiichi
Zitrin, Adi
Donahue, Megan
Medezinski, Elinor
Postman, Marc
Carrasco, Mauricio
Anguita, Timo
Geller, Margaret J.
Rines, Kenneth J.
Diaferio, Antonaldo
Kurtz, Michael J.
Bradley, Larry
Koekemoer, Anton
Zheng, Wei
Nonino, Mario
Molino, Alberto
Mahdavi, Andisheh
Lemze, Doron
Infante, Leopoldo
Ogaz, Sara
Melchior, Peter
Host, Ole
Ford, Holland
Grillo, Claudio
Rosati, Piero
Jimenez-Teja, Yolanda
Moustakas, John
Broadhurst, Tom
Ascaso, Begona
Lahav, Ofer
Bartelmann, Matthias
Benitez, Narciso
Bouwens, Rychard
Graur, Or
Graves, Genevieve
Jha, Saurabh
Jouvel, Stephanie
Kelson, Daniel
Moustakas, Leonidas
Maoz, Dan
Meneghetti, Massimo
Merten, Julian
Riess, Adam
Rodney, Steve
Seitz, Stella
TI CLASH: PRECISE NEW CONSTRAINTS ON THE MASS PROFILE OF THE GALAXY CLUSTER
A2261
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark energy; dark matter; galaxies: clusters: individual (Abell 2261);
galaxies: evolution; gravitational lensing: strong; gravitational
lensing: weak
ID DARK-MATTER HALOS; STRONG-LENSING ANALYSIS; HUBBLE-SPACE-TELESCOPE;
EXTREME-VALUE STATISTICS; LARGE-SCALE STRUCTURE; DEEP ADVANCED CAMERA;
DIGITAL SKY SURVEY; SIMILAR-TO 1; X-RAY; SUNYAEV-ZELDOVICH
AB We precisely constrain the inner mass profile of A2261 (z = 0.225) for the first time and determine that this cluster is not "overconcentrated" as found previously, implying a formation time in agreement with Lambda CDM expectations. These results are based on multiple strong-lensing analyses of new 16-band Hubble Space Telescope imaging obtained as part of the Cluster Lensing and Supernova survey with Hubble. Combining this with revised weak-lensing analyses of Subaru wide-field imaging with five-band Subaru + KPNO photometry, we place tight new constraints on the halo virial mass M-vir = (2.2 +/- 0.2) x 10(15) M-circle dot h(70)(-1) (within r(vir) approximate to 3 Mpc h(70)(-1)) and concentration c(vir) = 6.2 +/- 0.3 when assuming a spherical halo. This agrees broadly with average c(M, z) predictions from recent Lambda CDM simulations, which span 5 less than or similar to < c > less than or similar to 8. Our most significant systematic uncertainty is halo elongation along the line of sight (LOS). To estimate this, we also derive a mass profile based on archival Chandra X-ray observations and find it to be similar to 35% lower than our lensing-derived profile at r(2500) similar to 600 kpc. Agreement can be achieved by a halo elongated with a similar to 2:1 axis ratio along our LOS. For this elongated halo model, we find M-vir = (1.7 +/- 0.2) x 10(15) M-circle dot h(70)(-1) and c(vir) = 4.6 +/- 0.2, placing rough lower limits on these values. The need for halo elongation can be partially obviated by non-thermal pressure support and, perhaps entirely, by systematic errors in the X-ray mass measurements. We estimate the effect of background structures based on MMT/Hectospec spectroscopic redshifts and find that these tend to lower M-vir further by similar to 7% and increase c(vir) by similar to 5%.
C1 [Coe, Dan; Postman, Marc; Bradley, Larry; Koekemoer, Anton; Ogaz, Sara; Riess, Adam] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Zitrin, Adi; Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-6900 Heidelberg, Germany.
[Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Medezinski, Elinor; Zheng, Wei; Lemze, Doron; Ford, Holland; Riess, Adam; Rodney, Steve] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Carrasco, Mauricio; Anguita, Timo; Infante, Leopoldo] Pontificia Univ Catolica Chile, AIUC, Dept Astron & Astrophys, Santiago, Chile.
[Carrasco, Mauricio; Rosati, Piero] European So Observ, D-8046 Garching, Germany.
[Anguita, Timo] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Geller, Margaret J.; Rines, Kenneth J.; Kurtz, Michael J.] Smithsonian Astrophys Observ, Cambridge, MA USA.
[Rines, Kenneth J.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA.
[Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Turin, Italy.
[Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Nonino, Mario] Osserv Astron Trieste, Ist Nazl Astrofis, I-34131 Trieste, Italy.
[Molino, Alberto; Jimenez-Teja, Yolanda; Ascaso, Begona; Benitez, Narciso] Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Mahdavi, Andisheh] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Melchior, Peter] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Host, Ole; Lahav, Ofer; Jouvel, Stephanie] UCL, Dept Phys & Astron, London, England.
[Grillo, Claudio] Tech Univ Munich, Excellence Cluster Universe, D-8046 Garching, Germany.
[Moustakas, John] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92103 USA.
[Broadhurst, Tom] Univ Basque Country UPV EHU, Dept Theoret Phys, Bilbao, Spain.
[Broadhurst, Tom] Basque Fdn Sci, Ikerbasque, Bilbao, Spain.
[Bouwens, Rychard] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Graur, Or; Maoz, Dan] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Graves, Genevieve] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Jha, Saurabh] Rutgers State Univ, Dept Phys & Astron, New Brunswick, NJ 08903 USA.
[Kelson, Daniel] Carnegie Observ, Carnegie Inst Sci, Pasadena, CA USA.
[Moustakas, Leonidas; Merten, Julian] CALTECH, Jet Prop Lab, La Canada Flintridge, CA USA.
[Meneghetti, Massimo] Astron Observ Bologna, Ist Nazl Astrofis, Bologna, Italy.
[Seitz, Stella] Univ Sternwarte, Inst Astron, Munich, Germany.
[Seitz, Stella] Univ Sternwarte, Inst Astrophys, Munich, Germany.
RP Coe, D (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM DCoe@STScI.edu
RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014;
Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015;
Meneghetti, Massimo/O-8139-2015;
OI Benitez, Narciso/0000-0002-0403-7455; Koekemoer,
Anton/0000-0002-6610-2048; Grillo, Claudio/0000-0002-5926-7143;
Meneghetti, Massimo/0000-0003-1225-7084; Nonino,
Mario/0000-0001-6342-9662; Kurtz, Michael/0000-0002-6949-0090; Graur,
Or/0000-0002-4391-6137; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas,
Leonidas/0000-0003-3030-2360
FU NASA [NAS 5-26555, NAS 5-32864, HST-GO-12065.01-A]; National Science
Council of Taiwan [NSC100-2112-M-001-008-MY3]; Israel Science
Foundation; German Science Foundation [Transregio TR 33]; Spanish MICINN
[YA2010-22111-C03-00]; Junta de Andalucia Proyecto de Excelencia
[NBL2003]; INAF Contracts [ASI-INAF I/009/10/0, ASI-INAF I/023/05/0,
ASI-INAF I/088/06/0, PRIN INAF 2009, PRIN INAF 2010]; NSF [AST-0847157];
UK's STFC; Royal Society; Wolfson Foundation; Academia Sinica Career
Development Award; Internationale Spitzenforschung II-1 of the
Baden-Wurttemberg Stiftung; Smithsonian Institution; Cottrell College
Science Award from Research Corporation; INFN [PD51]; PRIN-MIUR
[2008NR3EBK_003]; Conicyt FONDAP/BASAL grant; DFG
FX The CLASH Multi-Cycle Treasury Program is based on observations made
with the NASA/ESA Hubble Space Telescope. The Space Telescope Science
Institute is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS 5-26555. ACS was developed
under NASA Contract NAS 5-32864.; This research is supported in part by
NASA Grant HST-GO-12065.01-A, National Science Council of Taiwan Grant
NSC100-2112-M-001-008-MY3, the Israel Science Foundation, the German
Science Foundation (Transregio TR 33), Spanish MICINN Grant
YA2010-22111-C03-00, funding from the Junta de Andalucia Proyecto de
Excelencia NBL2003, INAF Contracts ASI-INAF I/009/10/0, ASI-INAF
I/023/05/0, ASI-INAF I/088/06/0, PRIN INAF 2009, and PRIN INAF 2010, NSF
CAREER Grant AST-0847157, the UK's STFC, the Royal Society, and the
Wolfson Foundation. K. U. acknowledges support from the Academia Sinica
Career Development Award. A.Z. is supported by contract research
Internationale Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung.
M.J.G., K.J.R., A. D., and M.J.K. acknowledge partial support from the
Smithsonian Institution. K.J.R. was funded in part by a Cottrell College
Science Award from the Research Corporation. A. D. gratefully
acknowledges partial support from the INFN Grant PD51 and the
PRIN-MIUR-2008 Grant 2008NR3EBK_003 "Matter-antimatter asymmetry, dark
matter and dark energy in the LHC era." L. I. acknowledges support from
a Conicyt FONDAP/BASAL grant. P. R. and S. S. acknowledge support from
the DFG cluster of excellence Origin and Structure of the Universe
program.
NR 189
TC 57
Z9 57
U1 1
U2 19
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 22
DI 10.1088/0004-637X/757/1/22
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800022
ER
PT J
AU Currie, T
Rodigas, TJ
Debes, J
Plavchan, P
Kuchner, M
Jang-Condell, H
Wilner, D
Andrews, S
Kraus, A
Dahm, S
Robitaille, T
AF Currie, Thayne
Rodigas, Timothy J.
Debes, John
Plavchan, Peter
Kuchner, Marc
Jang-Condell, Hannah
Wilner, David
Andrews, Sean
Kraus, Adam
Dahm, Scott
Robitaille, Thomas
TI KECK/NIRC2 IMAGING OF THE WARPED, ASYMMETRIC DEBRIS DISK AROUND HD 32297
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: early-type; stars: individual (HD 32297)
ID SPITZER-SPACE-TELESCOPE; ORBITING HR 8799; BETA-PICTORIS B; MU-M;
CIRCUMSTELLAR DISK; PLANET FORMATION; RESONANT SIGNATURES;
OPTICAL-IMAGES; DUST DISK; HD-32297
AB We present Keck/NIRC2 K-s-band high-contrast coronagraphic imaging of the luminous debris disk around the nearby, young A star HD 32297 resolved at a projected separation of r = 0.'' 3-2.'' 5 (approximate to 35-280 AU). The disk is highly warped to the north and exhibits a complex, "wavy" surface brightness (SB) profile interior to r approximate to 110 AU, where the peaks/plateaus in the profiles are shifted between the NE and SW disk lobes. The SW side of the disk is 50%-100% brighter at r = 35-80 AU, and the location of its peak brightness roughly coincides with the disk's millimeter (mm) emission peak. Spectral energy distribution modeling suggests that HD 32297 has at least two dust populations that may originate from two separate belts, likely at different locations, possibly at distances coinciding with the SB peaks. A disk model for a single dust belt including a phase function with two components and a 5-10 AU pericenter offset explains the disk's warped structure and reproduces some of the SB profile's shape (e. g., the overall "wavy" profile, the SB peak/plateau shifts) but more poorly reproduces the disk's brightness asymmetry and the profile at wider separations (r > 110 AU). Although there may be alternate explanations, agreement between the SW disk brightness peak and disk's peak mm emission is consistent with an overdensity of very small, sub-blowout-sized dust and large, 0.1-1 mm sized grains at approximate to 45 AU tracing the same parent population of planetesimals. New near-IR and submillimeter observations may be able to clarify whether even more complex grain scattering properties or dynamical sculpting by an unseen planet are required to explain HD 32297's disk structure.
C1 [Currie, Thayne; Kuchner, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rodigas, Timothy J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Debes, John] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Plavchan, Peter] CALTECH, NEXSCI, Pasadena, CA 91125 USA.
[Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Wilner, David; Andrews, Sean] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kraus, Adam] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Robitaille, Thomas] MPIA Heidelberg, D-69117 Heidelberg, Germany.
RP Currie, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
OI Jang-Condell, Hannah/0000-0002-7639-1322; Rodigas,
Timothy/0000-0002-7535-2997; Robitaille, Thomas/0000-0002-8642-1329
FU NASA; W. M. Keck Foundation
FX We thank Richard Walters and Gregory Wirth for valuable help in setting
up these observations, which were conducted remotely from the California
Institute of Technology, and to Randy Campbell for indispensable NIRC2
support in helping the observer (T. C.) conduct his observations
efficiently. Karl Stapelfeldt, Scott Kenyon, and Margaret Moerchen
provided very useful discussions and the anonymous referee provided
helpful comments. T. C. is supported by a NASA Postdoctoral Fellowship.
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. We
acknowledge the significant cultural role and reverence that the Mauna
Kea summit has always had within the indigenous Hawaiian community. We
are grateful to be able to conduct observations from this mountain. 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.
NR 61
TC 21
Z9 21
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 28
DI 10.1088/0004-637X/757/1/28
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800028
ER
PT J
AU D'Angelo, G
Marzari, F
AF D'Angelo, Gennaro
Marzari, Francesco
TI OUTWARD MIGRATION OF JUPITER AND SATURN IN EVOLVED GASEOUS DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; hydrodynamics; methods: numerical;
planet-disk interactions; planets and satellites: formation;
protoplanetary disks
ID PASSIVE CIRCUMSTELLAR DISKS; PRIMORDIAL SOLAR NEBULA; GAS GIANT PLANETS;
X-RAY-RADIATION; T-TAURI STARS; ACCRETION DISKS; PROTOPLANETARY DISKS;
TIDAL INTERACTION; EXTREME-ULTRAVIOLET; VERTICAL STRUCTURE
AB The outward migration of a pair of resonant-orbit planets, driven by tidal interactions with a gas-dominated disk, is studied in the context of evolved solar nebula models. The planets' masses, M-1 and M-2, correspond to those of Jupiter and Saturn. Hydrodynamical calculations in two and three dimensions are used to quantify the migration rates and analyze the conditions under which the outward migration mechanism may operate. The planets are taken to be fully formed after 10(6) and before 3 x 10(6) years. The orbital evolution of the planets in an evolving disk is then calculated until the disk's gas is completely dissipated. Orbital locking in the 3:2 mean motion resonance may lead to outward migration under appropriate conditions of disk viscosity and temperature. However, resonance locking does not necessarily result in outward migration. This is the case, for example, if convergent migration leads to locking in the 2:1 mean motion resonance, as post-formation disk conditions seem to suggest. Accretion of gas on the planets may deactivate the outward migration mechanism by raising the mass ratio M-2/M-1 and/or by reducing the accretion rate toward the star, and hence depleting the inner disk. For migrating planets locked in the 3:2 mean motion resonance, there are stalling radii that depend on disk viscosity and on stellar irradiation, when it determines the disk's thermal balance. Planets locked in the 3:2 orbital resonance that start moving outward from within 1-2AU may reach beyond approximate to 5AU only under favorable conditions. However, within the explored space of disk parameters, only a small fraction-less than a few percent-of the models predict that the interior planet reaches beyond approximate to 4AU.
C1 [D'Angelo, Gennaro] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[D'Angelo, Gennaro] SETI Inst, Mountain View, CA 94043 USA.
[Marzari, Francesco] Univ Padua, Dept Phys, I-35131 Padua, Italy.
RP D'Angelo, G (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA.
EM gennaro.dangelo@nasa.gov; francesco.marzari@pd.infn.it
RI D'Angelo, Gennaro/L-7676-2014
OI D'Angelo, Gennaro/0000-0002-2064-0801
FU NASA [202844.02.02.01.75, NNX11AD20G, NNX11AK54G]
FX We thank the referee for a prompt response and helpful suggestions. G.
D. thanks the Los Alamos National Laboratory for its hospitality. G. D.
acknowledges support from NASA Outer Planets Research Program grant
202844.02.02.01.75 and from NASA Origins of Solar Systems Program grants
NNX11AD20G and NNX11AK54G. Resources supporting this work were provided
by the NASA High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center.
NR 93
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 50
DI 10.1088/0004-637X/757/1/50
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800050
ER
PT J
AU Kucera, TA
Gibson, SE
Schmit, DJ
Landi, E
Tripathi, D
AF Kucera, T. A.
Gibson, S. E.
Schmit, D. J.
Landi, E.
Tripathi, D.
TI TEMPERATURE AND EXTREME-ULTRAVIOLET INTENSITY IN A CORONAL PROMINENCE
CAVITY AND STREAMER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences
ID EUV IMAGING SPECTROMETER; ACTIVE-REGION LOOPS; TOTAL SOLAR ECLIPSE;
ATOMIC DATABASE; QUIET-SUN; ELEMENTAL ABUNDANCES; DENSITY STRUCTURE;
EMISSION-LINES; HINODE; CHIANTI
AB We analyze the temperature and EUV line emission of a coronal cavity and surrounding streamer in terms of a morphological forward model. We use a series of iron line ratios observed with the Hinode Extreme-ultraviolet Imaging Spectrograph (EIS) on 2007 August 9 to constrain temperature as a function of altitude in a morphological forward model of the streamer and cavity. We also compare model predictions to the EIS EUV line intensities and polarized brightness (pB) data from the Mauna Loa Solar Observatory (MLSO) Mark 4 K-coronameter. This work builds on earlier analysis using the same model to determine geometry of and density in the same cavity and streamer. The fit to the data with altitude-dependent temperature profiles indicates that both the streamer and cavity have temperatures in the range 1.4-1.7 MK. However, the cavity exhibits substantial substructure such that the altitude-dependent temperature profile is not sufficient to completely model conditions in the cavity. Coronal prominence cavities are structured by magnetism so clues to this structure are to be found in their plasma properties. These temperature substructures are likely related to structures in the cavity magnetic field. Furthermore, we find that the model overestimates the EUV line intensities by a factor of 4-10, without overestimating pB. We discuss this difference in terms of filling factors and uncertainties in density diagnostics and elemental abundances.
C1 [Kucera, T. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gibson, S. E.; Schmit, D. J.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Schmit, D. J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80305 USA.
[Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Tripathi, D.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
RP Kucera, TA (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
RI Landi, Enrico/H-4493-2011; Tripathi, Durgesh/D-9390-2012;
OI Tripathi, Durgesh/0000-0003-1689-6254; Kucera,
Therese/0000-0001-9632-447X
FU International Space Science Institute (ISSI); NASA SHP program; NASA;
NASA Earth and Space Science Fellowship program; National Science
Foundation; [NNX10AM17G]; [NNX11AC20G]
FX The authors thank the International Space Science Institute (ISSI) for
funding a Working Group on Coronal Cavities, where this work began. We
thank Judy Karpen, Jim Klimchuk, Adrian Daw, and Jack Ireland for
helpful conversations and Judy Karpen also for useful comments on the
manuscript. We thank the referee whose comments and questions led to a
substantially improved paper. T. K. was supported by a grant from the
NASA SHP program; E. L. by the NNX10AM17G, NNX11AC20G, and other NASA
grants; and D. S. by the NASA Earth and Space Science Fellowship
program. Hinode is a Japanese mission developed and launched by
ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as
international partners. It is operated by these agencies in cooperation
with ESA and NSC (Norway). SOHO is a mission of international
cooperation between ESA and NASA. The National Center for Atmospheric
Research is sponsored by the National Science Foundation. Chianti is a
collaborative project involving George Mason University, the University
of Michigan (USA), and the University of Cambridge (UK).
NR 47
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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 SEP 20
PY 2012
VL 757
IS 1
AR 73
DI 10.1088/0004-637X/757/1/73
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800073
ER
PT J
AU Luna, M
Diaz, AJ
Karpen, J
AF Luna, M.
Diaz, A. J.
Karpen, J.
TI THE EFFECTS OF MAGNETIC-FIELD GEOMETRY ON LONGITUDINAL OSCILLATIONS OF
SOLAR PROMINENCES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences; Sun: oscillations
ID MAGNETOHYDRODYNAMIC WAVES; MHD OSCILLATIONS; PERIODIC MOTION; CORONAL
LOOPS; FILAMENT
AB We investigate the influence of the geometry of the solar filament magnetic structure on the large-amplitude longitudinal oscillations. A representative filament flux tube is modeled as composed of a cool thread centered in a dipped part with hot coronal regions on either side. We have found the normal modes of the system and establish that the observed longitudinal oscillations are well described with the fundamental mode. For small and intermediate curvature radii and moderate to large density contrast between the prominence and the corona, the main restoring force is the solar gravity. In this full wave description of the oscillation a simple expression for the oscillation frequencies is derived in which the pressure-driven term introduces a small correction. We have also found that the normal modes are almost independent of the geometry of the hot regions of the tube. We conclude that observed large-amplitude longitudinal oscillations are driven by the projected gravity along the flux tubes and are strongly influenced by the curvature of the dips of the magnetic field in which the threads reside.
C1 [Luna, M.] CRESST, Greenbelt, MD 20771 USA.
[Luna, M.] NASA GSFC, Space Weather Lab, Greenbelt, MD 20771 USA.
[Diaz, A. J.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Diaz, A. J.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
RP Luna, M (reprint author), CRESST, Greenbelt, MD 20771 USA.
FU NASA Heliophysics SRT program; University of Maryland at College Park;
Spanish Ministry of Science [AYA2010-18029]
FX This work has been supported by the NASA Heliophysics SR&T program. M.L.
also acknowledges support from the University of Maryland at College
Park and the people of CRESST. A.J.D. acknowledges the financial support
by the Spanish Ministry of Science through project AYA2010-18029.
NR 29
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U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 98
DI 10.1088/0004-637X/757/1/98
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800098
ER
PT J
AU Miller, JM
Pooley, GG
Fabian, AC
Nowak, MA
Reis, RC
Cackett, EM
Pottschmidt, K
Wilms, J
AF Miller, J. M.
Pooley, G. G.
Fabian, A. C.
Nowak, M. A.
Reis, R. C.
Cackett, E. M.
Pottschmidt, K.
Wilms, J.
TI ON THE ROLE OF THE ACCRETION DISK IN BLACK HOLE DISK-JET CONNECTIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; relativistic processes;
X-rays: binaries
ID X-RAY BINARIES; ACTIVE GALACTIC NUCLEUS; BROAD-BAND SPECTRUM; NOVA
MUSCAE 1991; LOW-HARD STATE; CYGNUS X-1; LOW/HARD STATE; STRONG GRAVITY;
IRON-LINE; DOMINATED ACCRETION
AB Models of jet production in black hole systems suggest that the properties of the accretion disk-such as its mass accretion rate, inner radius, and emergent magnetic field-should drive and modulate the production of relativistic jets. Stellar-mass black holes in the "low/hard" state are an excellent laboratory in which to study disk-jet connections, but few coordinated observations are made using spectrometers that can incisively probe the inner disk. We report on a series of 20 Suzaku observations of Cygnus X-1 made in the jet-producing low/hard state. Contemporaneous radio monitoring was done using the Arcminute MicroKelvin Array radio telescope. Two important and simple results are obtained: (1) the jet (as traced by radio flux) does not appear to be modulated by changes in the inner radius of the accretion disk and (2) the jet is sensitive to disk properties, including its flux, temperature, and ionization. Some more complex results may reveal aspects of a coupled disk-corona-jet system. A positive correlation between the reflected X-ray flux and radio flux may represent specific support for a plasma ejection model of the corona, wherein the base of a jet produces hard X-ray emission. Within the framework of the plasma ejection model, the spectra suggest a jet base with v/c similar or equal to 0.3 or the escape velocity for a vertical height of z similar or equal to 20 GM/c(2) above the black hole. The detailed results of X-ray disk continuum and reflection modeling also suggest a height of z similar or equal to 20 GM/c(2) for hard X-ray production above a black hole, with a spin in the range 0.6 <= a <= 0.99. This height agrees with X-ray time lags recently found in Cygnus X-1. The overall picture that emerges from this study is broadly consistent with some jet-focused models for black hole spectral energy distributions in which a relativistic plasma is accelerated at z = 10-100 GM/c(2). We discuss these results in the context of disk-jet connections across the black hole mass scale.
C1 [Miller, J. M.; Reis, R. C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Pooley, G. G.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Fabian, A. C.; Cackett, E. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Nowak, M. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Wilms, J.] Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM jonmm@umich.edu
RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009;
OI Wilms, Joern/0000-0003-2065-5410; reis, rubens/0000-0002-6618-2412
NR 105
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U1 0
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 11
DI 10.1088/0004-637X/757/1/11
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800011
ER
PT J
AU Morales, FY
Padgett, DL
Bryden, G
Werner, MW
Furlan, E
AF Morales, Farisa Y.
Padgett, D. L.
Bryden, G.
Werner, M. W.
Furlan, E.
TI WISE DETECTIONS OF DUST IN THE HABITABLE ZONES OF PLANET-BEARING STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: planetary systems; planets and
satellites: formation; stars: individual (UScoCTIO 108)
ID SOLAR-TYPE STARS; SPITZER-SPACE-TELESCOPE; SPECTRAL
ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; DEBRIS
DISKS; UPPER SCORPIUS; BETA-PICTORIS; MIPS SURVEY; K-GIANT
AB We use data from the Wide-field Infrared Survey Explorer (WISE) all-sky release to explore the incidence of warm dust in the habitable zones around exoplanet-host stars. Dust emission at 12 and/or 22 mu m (T-dust similar to 300 and/or similar to 150 K) traces events in the terrestrial planet zones; its existence implies replenishment by evaporation of comets or collisions of asteroids, possibly stirred by larger planets. Of the 591 planetary systems (728 extrasolar planets) in the Exoplanet Encyclopaedia as of 2012 January 31, 350 are robustly detected by WISE at >= 5 sigma level. We perform detailed photosphere subtraction using tools developed for Spitzer data and visually inspect all the WISE images to confirm bona fide point sources. We find nine planet-bearing stars show dust excess emission at 12 and/or 22 mu m at >= 3 sigma level around young, main-sequence, or evolved giant stars. Overall, our results yield an excess incidence of similar to 2.6% for stars of all evolutionary stages, but similar to 1% for planetary debris disks around main-sequence stars. Besides recovering previously known warm systems, we identify one new excess candidate around the young star UScoCTIO 108.
C1 [Morales, Farisa Y.; Bryden, G.; Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Padgett, D. L.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Furlan, E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Morales, FY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Farisa@jpl.nasa.gov
OI Furlan, Elise/0000-0001-9800-6248
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration
FX The research described in this publication was carried out with internal
R&TD funding at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. This publication makes use of data products from the Two
Micron All Sky Survey (2MASS) and from the SIMBAD Web site. This
publication also makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This research has made use of the NASA Exoplanet
Archive, which is operated by the California Institute of Technology,
under contract with the National Aeronautics and Space Administration
under the Exoplanet Exploration Program.
NR 43
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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 SEP 20
PY 2012
VL 757
IS 1
AR 7
DI 10.1088/0004-637X/757/1/7
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800007
ER
PT J
AU Pongkitiwanichakul, P
Chandran, BDG
Karpen, JT
DeVore, CR
AF Pongkitiwanichakul, Peera
Chandran, Benjamin D. G.
Karpen, Judith T.
DeVore, C. Richard
TI THE EFFECTS OF WAVE ESCAPE ON FAST MAGNETOSONIC WAVE TURBULENCE IN SOLAR
FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE plasmas; Sun: corona; Sun: flares; waves
ID PARTICLE-ACCELERATION; DYNAMICS; FLOWS
AB One of the leading models for electron acceleration in solar flares is stochastic acceleration by weakly turbulent fast magnetosonic waves ("fast waves"). In this model, large-scale flows triggered by magnetic reconnection excite large-wavelength fast waves, and fast-wave energy then cascades from large wavelengths to small wavelengths. Electron acceleration by large-wavelength fast waves is weak, and so the model relies on the small-wavelength waves produced by the turbulent cascade. In order for the model to work, the energy cascade time for large-wavelength fast waves must be shorter than the time required for the waves to propagate out of the solar-flare acceleration region. To investigate the effects of wave escape, we solve the wave kinetic equation for fast waves in weak turbulence theory, supplemented with a homogeneous wave-loss term. We find that the amplitude of large-wavelength fast waves must exceed a minimum threshold in order for a significant fraction of the wave energy to cascade to small wavelengths before the waves leave the acceleration region. We evaluate this threshold as a function of the dominant wavelength of the fast waves that are initially excited by reconnection outflows.
C1 [Pongkitiwanichakul, Peera; Chandran, Benjamin D. G.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Pongkitiwanichakul, Peera; Chandran, Benjamin D. G.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Karpen, Judith T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[DeVore, C. Richard] USN, Res Lab, Washington, DC 20375 USA.
RP Pongkitiwanichakul, P (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
EM pbu3@unh.edu; benjamin.chandran@unh.edu; judy.karpen@nasa.gov;
devore@nrl.navy.mil
RI DeVore, C/A-6067-2015
OI DeVore, C/0000-0002-4668-591X
FU NASA [NNX07AP65G, NNX11AJ37G]; NSF [AGS-0851005]; DOE
[DE-FG02-07-ER46372]; NSF/DOE [AGS-1003451]
FX This work benefited from valuable discussions with our colleagues in a
NASA Living-With-a-Star Focused-Science-Topic team working on "Flare
Particle Acceleration Near the Sun and Contribution to Large SEP
Events." This work was supported in part by NASA grants NNX07AP65G and
NNX11AJ37G, NSF grant , DOE grant DE-FG02-07-ER46372, and NSF/DOE grant
AGS-1003451.
NR 24
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 72
DI 10.1088/0004-637X/757/1/72
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800072
ER
PT J
AU Pueyo, L
Hillenbrand, L
Vasisht, G
Oppenheimer, BR
Monnier, JD
Hinkley, S
Crepp, J
Roberts, LC
Brenner, D
Zimmerman, N
Parry, I
Beichman, C
Dekany, R
Shao, M
Burruss, R
Cady, E
Roberts, J
Soummer, R
AF Pueyo, Laurent
Hillenbrand, Lynne
Vasisht, Gautam
Oppenheimer, Ben R.
Monnier, John D.
Hinkley, Sasha
Crepp, Justin
Roberts, Lewis C., Jr.
Brenner, Douglas
Zimmerman, Neil
Parry, Ian
Beichman, Charles
Dekany, Richard
Shao, Mike
Burruss, Rick
Cady, Eric
Roberts, Jenny
Soummer, Remi
TI CONSTRAINING MASS RATIO AND EXTINCTION IN THE FU ORIONIS BINARY SYSTEM
WITH INFRARED INTEGRAL FIELD SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: visual; stars: individual (FU Orionis); stars: protostars;
techniques: high angular resolution; techniques: imaging spectroscopy
ID YOUNG STELLAR OBJECTS; ADAPTIVE OPTICS SYSTEM; ACCRETION DISK; V1057
CYGNI; STARS; PHOTOMETRY; SPECTROGRAPH; EVOLUTION; PROTOSTELLAR;
CORONAGRAPHS
AB We report low-resolution near-infrared spectroscopic observations of the eruptive star FU Orionis using the Integral Field Spectrograph (IFS) Project 1640 installed at the Palomar Hale telescope. This work focuses on elucidating the nature of the faint source, located 0 ''.5 south of FU Ori, and identified in 2003 as FU Ori S. We first use our observations in conjunction with published data to demonstrate that the two stars are indeed physically associated and form a true binary pair. We then proceed to extract J- and H-band spectro-photometry using the damped LOCI algorithm, a reduction method tailored for high contrast science with IFS. This is the first communication reporting the high accuracy of this technique, pioneered by the Project 1640 team, on a faint astronomical source. We use our low-resolution near-infrared spectrum in conjunction with 10.2 mu m interferometric data to constrain the infrared excess of FU Ori S. We then focus on estimating the bulk physical properties of FU Ori S. Our models lead to estimates of an object heavily reddened, A(V) = 8-12, with an effective temperature of similar to 4000-6500 K. Finally, we put these results in the context of the FU Ori N-S system and argue that our analysis provides evidence that FU Ori S might be the more massive component of this binary system.
C1 [Pueyo, Laurent] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, Baltimore, MD 21218 USA.
[Pueyo, Laurent; Soummer, Remi] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hillenbrand, Lynne; Hinkley, Sasha; Dekany, Richard; Roberts, Jenny] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Vasisht, Gautam; Roberts, Lewis C., Jr.; Shao, Mike; Burruss, Rick; Cady, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Oppenheimer, Ben R.; Brenner, Douglas; Zimmerman, Neil] Amer Museum Nat Hist, New York, NY 10024 USA.
[Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Crepp, Justin] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Parry, Ian] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Beichman, Charles] NASA Exoplanet Sci Inst, Pasadena, CA 91225 USA.
RP Pueyo, L (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, 3400 N Charles St, Baltimore, MD 21218 USA.
OI Roberts, Lewis/0000-0003-3892-2900; Zimmerman, Neil/0000-0001-5484-1516
FU National Aeronautics and Space Administration; National Science
Foundation [AST-0520822, AST-0804417, AST-0908484]; NASA ROSES Origins
of Solar Systems [NMO710830/102190]; NSF [AST-0908497, AST-0619922,
AST-1007046]; JPL; Caltech; NASA; California Institute of Technology
(Caltech); NASA through the Sagan Fellowship Program
FX The research described in this publication was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Project
1640 is funded by National Science Foundation grants AST-0520822,
AST-0804417, and AST-0908484. This work was partially funded through the
NASA ROSES Origins of Solar Systems Grant NMO710830/102190, the NSF
AST-0908497 Grant. The adaptive optics program at Palomar is supported
by NSF grants AST-0619922 and AST-1007046. L. P. was supported by an
appointment to the NASA Postdoctoral Program at the JPL, Caltech,
administered by Oak Ridge Associated Universities through a contract
with NASA. L. P. and S. H. performed this work in part under contract
with the California Institute of Technology (Caltech) funded by NASA
through the Sagan Fellowship Program. This work was based in part on
data collected at the Subaru Telescope and obtained from the SMOKA,
which is operated by the Astronomy Data Center, National Observatory of
Japan.
NR 56
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 57
DI 10.1088/0004-637X/757/1/57
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800057
ER
PT J
AU Robinson, TD
Catling, DC
AF Robinson, Tyler D.
Catling, David C.
TI AN ANALYTIC RADIATIVE-CONVECTIVE MODEL FOR PLANETARY ATMOSPHERES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE convection; radiation mechanisms: general; planets and satellites:
atmospheres; planets and satellites: general
ID THERMAL EQUILIBRIUM; VENUS MESOSPHERE; TITAN; TEMPERATURE; GREENHOUSE;
GRAY; JUPITER; METHANE; SURFACE; CLOUDS
AB We present an analytic one-dimensional radiative-convective model of the thermal structure of planetary atmospheres. Our model assumes that thermal radiative transfer is gray and can be represented by the two-stream approximation. Model atmospheres are assumed to be in hydrostatic equilibrium, with a power-law scaling between the atmospheric pressure and the gray thermal optical depth. The convective portions of our models are taken to follow adiabats that account for condensation of volatiles through a scaling parameter to the dry adiabat. By combining these assumptions, we produce simple, analytic expressions that allow calculations of the atmospheric-pressure-temperature profile, as well as expressions for the profiles of thermal radiative flux and convective flux. We explore the general behaviors of our model. These investigations encompass (1) worlds where atmospheric attenuation of sunlight is weak, which we show tend to have relatively high radiative-convective boundaries; (2) worlds with some attenuation of sunlight throughout the atmosphere, which we show can produce either shallow or deep radiative-convective boundaries, depending on the strength of sunlight attenuation; and (3) strongly irradiated giant planets (including hot Jupiters), where we explore the conditions under which these worlds acquire detached convective regions in their mid-tropospheres. Finally, we validate our model and demonstrate its utility through comparisons to the average observed thermal structure of Venus, Jupiter, and Titan, and by comparing computed flux profiles to more complex models.
C1 [Robinson, Tyler D.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Catling, David C.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Robinson, Tyler D.; Catling, David C.] NASA, Astrobiol Inst, Virtual Planetary Lab, Washington, DC USA.
[Robinson, Tyler D.; Catling, David C.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
RP Robinson, TD (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM robinson@astro.washington.edu
OI Catling, David/0000-0001-5646-120X
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNH05ZDA001C]
FX This work was performed as part of the NASA Astrobiology Institute's
Virtual Planetary Laboratory, supported by the National Aeronautics and
Space Administration through the NASA Astrobiology Institute under
solicitation No. NNH05ZDA001C. We thank David Crisp, Kevin Zahnle,
Jonathan Fortney, Tristan Guillot, Vivien Parmentier, and the late
Conway Leovy for discussions and insights provided during this project.
We also thank Ray Pierrehumbert for an insightful and friendly review.
NR 52
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2012
VL 757
IS 1
AR 104
DI 10.1088/0004-637X/757/1/104
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800104
ER
PT J
AU Schmelz, JT
Kimble, JA
Saba, JLR
AF Schmelz, J. T.
Kimble, J. A.
Saba, J. L. R.
TI DERIVING PLASMA DENSITIES AND ELEMENTAL ABUNDANCES FROM SERTS
DIFFERENTIAL EMISSION MEASURE ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: abundances; Sun: corona; Sun: fundamental parameters; Sun: UV
radiation; Sun: X-rays, gamma rays
ID X-RAY TELESCOPE; EXTREME-ULTRAVIOLET SPECTRA; SOLAR ACTIVE-REGION;
ENERGETIC PARTICLES; IONIZATION EQUILIBRIUM; CORONAL ABUNDANCES; ATOMIC
DATABASE; SPECTROMETER; ATMOSPHERE; CALCIUM
AB We use high-resolution spectral emission line data obtained by the SERTS instrument during three rocket flights to demonstrate a new approach for constraining electron densities of solar active region plasma. We apply differential emission measure (DEM) forward-fitting techniques to characterize the multithermal solar plasma producing the observed EUV spectra, with constraints on the high-temperature plasma from the Yohkoh Soft X-ray Telescope. In this iterative process, we compare line intensities predicted by an input source distribution to observed line intensities for multiple iron ion species, and search a broad range of densities to optimize chi(2) simultaneously for the many available density-sensitive lines. This produces a density weighted by the DEM, which appears to be useful for characterizing the bulk of the emitting plasma over a significant range of temperature. This "DEM-weighted density" technique is complementary to the use of density-sensitive line ratios and less affected by uncertainties in atomic data and ionization fraction for any specific line. Once the DEM shape and the DEM-weighted density have been established from the iron lines, the relative elemental abundances can be determined for other lines in the spectrum. We have also identified spectral lines in the SERTS wavelength range that may be problematic.
C1 [Schmelz, J. T.; Kimble, J. A.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
[Saba, J. L. R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Saba, J. L. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
EM jschmelz@memphis.edu
FU NASA/SAO; NSF [ATM-0402729]; small Yohkoh Guest Investigator grant
FX CHIANTI is a collaborative project involving the NRL (USA), the
Universities of Florence (Italy) and Cambridge (UK), and George Mason
University (USA). Solar physics research at the University of Memphis is
supported by a Hinode subcontract from NASA/SAO as well as NSF
ATM-0402729. The impetus for this work was a pilot study funded by a
small Yohkoh Guest Investigator grant.
NR 41
TC 3
Z9 3
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 SEP 20
PY 2012
VL 757
IS 1
AR 17
DI 10.1088/0004-637X/757/1/17
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800017
ER
PT J
AU Verkhoglyadova, OP
Li, G
Ao, X
Zank, GP
AF Verkhoglyadova, O. P.
Li, G.
Ao, X.
Zank, G. P.
TI RADIAL DEPENDENCE OF PEAK PROTON AND IRON ION FLUXES IN SOLAR ENERGETIC
PARTICLE EVENTS: APPLICATION OF THE PATH CODE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; shock waves; solar-terrestrial relations;
Sun: coronal mass ejections (CMEs); Sun: heliosphere
ID EJECTION-DRIVEN SHOCKS; CORONAL MASS EJECTIONS; INTERPLANETARY SHOCKS;
SEP EVENTS; INNER HELIOSPHERE; HIGH-ENERGIES; ACCELERATION; TRANSPORT;
FLUENCES; SPACE
AB The radial dependence of particle peak fluxes in large solar energetic particle (SEP) events is important in determining the potential impact of space weather hazards on space missions. Using the Particle Acceleration and Transport in the Heliosphere code, we model the acceleration and transport of protons and iron ions at evolving coronal mass ejection shocks propagating throughout the inner heliosphere from about 0.1 to 2.5 AU. An example shock with a compression ratio of 3.9 and a speed of 1000 km s(-1) close to the Sun is modeled using a two-dimensional MHD ZEUS code. The compression ratio and shock speed weakened to 2.3 and 630 km s(-1), correspondingly, at 2 AU. Shocks with 15 degrees, 45 degrees, and 75 degrees angles between the upstream magnetic field and the shock normal were studied. The shock angle was kept constant throughout the simulation. Both gradual and impulsive events are studied. Diffusive shock acceleration is assumed at the shock and we use a total diffusion coefficient that includes a parallel diffusion coefficient which takes into account the upstream wave amplification, and a perpendicular diffusion coefficient which is based on the NonLinear Guiding Center theory. The transport of particles escaping from the shock is modeled using a Monte Carlo approach. Time-intensity profiles for protons and iron ions are obtained. We analyzed the radial dependence of peak fluxes (J) for both protons and iron ions from 0.5 to 2 AU. We find that the functional dependence is softer than R-3 and is about R-2.9 to R-1.8 in the energy range of 0.3-5 MeV nuc(-1). Quasi-perpendicular shock showed a steeper radial dependence than a quasi-parallel shock. Mixed events show a softer radial dependence at energies above 500 keV nuc(-1) for iron ions and above 1 MeV for protons. The values of J (R) depend on seed particle composition, particle energy, shock obliquity, and the interplanetary turbulence level. Consequently, we advocate using SEP event-specific computer modeling rather than empirical formulae for future forecasting of the radiation environment throughout the heliosphere during large SEP events.
C1 [Verkhoglyadova, O. P.; Li, G.; Ao, X.; Zank, G. P.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Verkhoglyadova, O. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Li, G.; Zank, G. P.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
RP Verkhoglyadova, OP (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
RI Li, Gang/B-4977-2012;
OI Li, Gang/0000-0003-4695-8866; Verkhoglyadova, Olga/0000-0002-9295-9539
FU NSF [SHINE: AGS-0962658]; NASA [NNX09AG70G, NNX09AJ79G, ATM-0904007,
NNX09AP74A, FA9550-10-1-0084, NNX09AW45G, 12-036]
FX The authors acknowledge the partial support of NSF SHINE: AGS-0962658
and NASA grants NNX09AG70G, NNX09AJ79G, ATM-0904007, NNX09AP74A,
FA9550-10-1-0084, NNX09AW45G, EMMREM Subaward # 12-036, PO 13390.
NR 45
TC 18
Z9 18
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 SEP 20
PY 2012
VL 757
IS 1
AR 75
DI 10.1088/0004-637X/757/1/75
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800075
ER
PT J
AU Younes, G
Kouveliotou, C
Kargaltsev, O
Pavlov, GG
Gogus, E
Wachter, S
AF Younes, G.
Kouveliotou, C.
Kargaltsev, O.
Pavlov, G. G.
Gogus, E.
Wachter, S.
TI XMM-NEWTON VIEW OF SWIFT J1834.9-0846 AND ITS MAGNETAR WIND NEBULA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: neutron; X-rays: individual (Swift J1834.9-0846); X-rays: ISM
ID SOFT-GAMMA-REPEATER; X-RAY-EMISSION; 2004 DECEMBER 27; RADIO PULSAR
J1119-6127; GIANT FLARE; NEUTRON-STARS; SGR 1806-20; XTE J1810-197;
INTERSTELLAR GRAINS; TRANSIENT MAGNETAR
AB We report on the analysis of two XMM-Newton observations of the recently discovered soft gamma repeater Swift J1834.9-0846, taken in 2005 September and one month after the source went into outburst on 2011 August 7. We performed timing and spectral analyses on the point source as well as on the extended emission. We find that the source period is consistent with an extrapolation of the Chandra ephemeris reported earlier and the spectral properties remained constant. The source luminosity decreased to a level of 1.6 x 10(34) erg s(-1) following a decay trend of proportional to t(-0.5). Our spatial analysis of the source environment revealed the presence of two extended emission regions around the source. The first (region A) is a symmetric ring around the point source, starting at 25 '' and extending to similar to 50 ''. We argue that region A is a dust scattering halo. The second (region B) has an asymmetrical shape extending between 50 '' and 150 '', and is detected both in the pre- and post-outburst data. We argue that this region is a possible magnetar wind nebula (MWN). The X-ray efficiency of the MWN with respect to the rotation energy loss is substantially higher than those of rotation-powered pulsars: eta(X) equivalent to L-MWN,L-0.5-8 keV/(E)over dot(rot) approximate to 0.7. The higher efficiency points to a different energy source for the MWN of Swift J1834.9-0846, most likely bursting activity of the magnetar, powered by its high magnetic field, B = 1.4 x 10(14) G.
C1 [Younes, G.] Univ Space Res Assoc, Huntsville, AL 35806 USA.
[Younes, G.; Kouveliotou, C.] NSSTC, Huntsville, AL 35805 USA.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA.
[Kargaltsev, O.] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA.
[Pavlov, G. G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Pavlov, G. G.] St Petersburg State Polytech Univ, St Petersburg 195251, Russia.
[Gogus, E.] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
[Wachter, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
RP Younes, G (reprint author), Univ Space Res Assoc, 6767 Old Madison Pike NW,Suite 450, Huntsville, AL 35806 USA.
FU ESA Member States; USA (NASA); NASA [NNX09AC81G, NNX09AC84G]; NSF
[AST09-08733, AST09-08611]; Ministry of Education and Science of the
Russian Federation [11.G34.31.0001]
FX This work is based on observations with XMM-Newton an ESA science
mission with instruments and contributions directly funded by ESA Member
States and the USA (NASA). The work by O.Y.K. and G. G. P. was partly
supported by NASA grants NNX09AC81G and NNX09AC84G, NSF grants
AST09-08733 and AST09-08611, and by the Ministry of Education and
Science of the Russian Federation (contract 11.G34.31.0001). The authors
are grateful to Norbert Schartel for his decision to allocate XMM-Newton
TOO time for observation of Swift J1834.9-0846. The authors thank the
referee for the constructive comments that helped improve the quality of
the manuscript.
NR 67
TC 19
Z9 19
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 SEP 20
PY 2012
VL 757
IS 1
AR 39
DI 10.1088/0004-637X/757/1/39
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009VG
UT WOS:000309052800039
ER
PT J
AU Molnar, L
Kollath, Z
Szabo, R
Bryson, S
Kolenberg, K
Mullally, F
Thompson, SE
AF Molnar, L.
Kollath, Z.
Szabo, R.
Bryson, S.
Kolenberg, K.
Mullally, F.
Thompson, S. E.
TI NONLINEAR ASTEROSEISMOLOGY OF RR LYRAE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: individual (RR Lyr); stars: oscillations; stars: variables: RR
Lyrae
ID KEPLER; STARS; PULSATION; CEPHEID; MODELS
AB The observations of the Kepler Space Telescope revealed that fundamental-mode RR Lyrae stars may show various radial overtones. The presence of multiple radial modes may allow us to conduct nonlinear asteroseismology: comparison of mode amplitudes and frequency shifts between observations and models. Here we report the detection of three radial modes in the star RR Lyr, the eponym of the class, using the Kepler short cadence data: besides the fundamental mode, both the first and the ninth overtones can be derived from the data set. RR Lyrae shows period doubling, but switches occasionally to a state where a pattern of six pulsation cycles repeats instead of two. We found hydrodynamic models that show the same three modes and the period-six state, allowing for comparison with the observations.
C1 [Molnar, L.; Kollath, Z.; Szabo, R.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary.
[Bryson, S.; Mullally, F.; Thompson, S. E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kolenberg, K.] Katholieke Univ Leuven, Inst Astron, B-3001 Heverlee, Belgium.
[Mullally, F.; Thompson, S. E.] SETI Inst, Mountain View, CA 94043 USA.
RP Molnar, L (reprint author), MTA CSFK, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary.
EM molnar.laszlo@csfk.mta.hu
OI Szabo, Robert/0000-0002-3258-1909; Molnar, Laszlo/0000-0002-8159-1599
FU NASA's Science Mission Directorate; Hungarian OTKA [K83790, K81421,
MB08C 81013]; "Lendulet" programme, and the European Community's Seventh
Framework Programme (FP7) [269194]; Hungarian Academy of Sciences; Marie
Curie International Outgoing Fellowship within the 7th European
Community Framework Programme; National Science Foundation [NSF
PHY05-51164]
FX Funding for this Discovery Mission is provided by NASA's Science Mission
Directorate. The Kepler Team and the Kepler Guest Observer Office are
recognized for helping to make the mission and these data possible. This
work was supported by the Hungarian OTKA grants K83790, K81421, and
MB08C 81013, as well as the "Lendulet" programme, and the European
Community's Seventh Framework Programme (FP7/2007-2013) under grant
agreement No. 269194. R.Sz. acknowledges the Bolyai Janos Scholarship of
the Hungarian Academy of Sciences. K.K. is supported by a Marie Curie
International Outgoing Fellowship within the 7th European Community
Framework Programme. R.Sz. and K.K. warmly thank the KITP staff of UCSB
for their hospitality during the "Asteroseismology in the Space Age"
programme. This research was supported in part by the National Science
Foundation under grant No. NSF PHY05-51164.
NR 23
TC 15
Z9 15
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 SEP 20
PY 2012
VL 757
IS 1
AR L13
DI 10.1088/2041-8205/757/1/L13
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 007VQ
UT WOS:000308916900013
ER
PT J
AU Washimi, H
Webber, W
Zank, GP
Hu, Q
Florinski, V
Adams, J
Kubo, Y
AF Washimi, H.
Webber, W.
Zank, G. P.
Hu, Q.
Florinski, V.
Adams, J.
Kubo, Y.
TI A ROLE OF MAGNETOSONIC PULSES ON VARIATIONS OF VOYAGER-1 MeV ELECTRON
INTENSITY IN THE HELIOSHEATH
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmic rays; interplanetary medium; ISM: kinematics and dynamics; ISM:
structure; solar wind; Sun: heliosphere
ID TERMINATION-SHOCK; MHD
AB Voyager 1 (V1) spacecraft observed electrons of 6-14 MeV in the heliosheath which showed several enhancements of significant flux variation. We compare these temporal electron flux variations, from the time when V1 crossed the termination shock (TS) up to mid-2008, with dynamical phenomena in the heliosheath that are obtained from our MHD simulations which are based on Voyager 2 (V2) observed solar-wind data. Our simulations indicate that all electron flux enhancements, except for one, correspond fairly well to the times when a magnetosonic (MS) pulse was driven downstream of the TS due to collision of interplanetary shock (IPS) or shock-driven MS pulse and its reflection in the heliosheath that either passed V1, or collided with the TS or with the plasma sheet near the heliopause (HP). This result suggests that these enhancements in the electron flux should correspond to either direct or indirect effects of MS pulses in the heliosheath driven by IPSs. The scale of the heliosphere is estimated by comparing V1-observed magnetic field intensity with the simulated intensity which suggests that V1 is possibly located near the HP within 4-8 AU at the present time.
C1 [Washimi, H.; Zank, G. P.; Hu, Q.; Florinski, V.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Webber, W.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Adams, J.] NASA MSFC, Huntsville, AL 35899 USA.
[Kubo, Y.] Natl Inst Informat & Commun Technol, Koganei, Tokyo 1848795, Japan.
RP Washimi, H (reprint author), Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
EM hw0002@uah.edu
FU NASA grants [NNG05EC85C, NNX09AW46G, NNX09AB40G, NNX09AW45G, NNM11AA01A]
FX We used the solar wind data from the MIT plasma experiment on V2 during
the period from DOY 253, 2001 to DOY 241, 2007, and NASA COHOweb data of
the V1-observed magnetic field in year 2006. We thank A. Kawamura for
graphic support. We acknowledge the support of NASA grants NNG05EC85C,
NNX09AW46G, NNX09AB40G, NNX09AW45G, and NNM11AA01A.
NR 9
TC 3
Z9 3
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 SEP 20
PY 2012
VL 757
IS 1
AR L2
DI 10.1088/2041-8205/757/1/L2
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 007VQ
UT WOS:000308916900002
ER
PT J
AU Wirstrom, ES
Charnley, SB
Cordiner, MA
Milam, SN
AF Wirstroem, Eva S.
Charnley, Steven B.
Cordiner, Martin A.
Milam, Stefanie N.
TI ISOTOPIC ANOMALIES IN PRIMITIVE SOLAR SYSTEM MATTER:
SPIN-STATE-DEPENDENT FRACTIONATION OF NITROGEN AND DEUTERIUM IN
INTERSTELLAR CLOUDS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: clouds; ISM: molecules; meteorites, meteors,
meteoroids; molecular processes; planets and satellites: formation
ID INTERPLANETARY DUST PARTICLES; TO-PARA RATIO; HYDROGEN-CYANIDE;
ORGANIC-MATTER; DARK CLOUDS; PRESTELLAR CORES; N-14/N-15 RATIO; DENSE
CORES; METEORITES; CHEMISTRY
AB Organic material found in meteorites and interplanetary dust particles is enriched in D and N-15. This is consistent with the idea that the functional groups carrying these isotopic anomalies, nitriles and amines, were formed by ion-molecule chemistry in the protosolar nebula. Theoretical models of interstellar fractionation at low temperatures predict large enrichments in both D and N-15 and can account for the largest isotopic enrichments measured in carbonaceous meteorites. However, more recent measurements have shown that, in some primitive samples, a large N-15 enrichment does not correlate with one in D, and that some D-enriched primitive material displays little, if any, N-15 enrichment. By considering the spin-state dependence in ion-molecule reactions involving the ortho and para forms of H-2, we show that ammonia and related molecules can exhibit such a wide range of fractionation for both N-15 and D in dense cloud cores. We also show that while the nitriles, HCN and HNC, contain the greatest N-15 enrichment, this is not expected to correlate with extreme D enrichment. These calculations therefore support the view that solar system N-15 and D isotopic anomalies have an interstellar heritage. We also compare our results to existing astronomical observations and briefly discuss future tests of this model.
C1 [Wirstroem, Eva S.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20770 USA.
NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20770 USA.
[Wirstroem, Eva S.; Cordiner, Martin A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Wirstrom, ES (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20770 USA.
EM ewirstrom@gmail.com
RI Milam, Stefanie/D-1092-2012;
OI Milam, Stefanie/0000-0001-7694-4129; Wirstrom, Eva/0000-0002-0656-876X
FU NASA's Origins of Solar Systems Program; Goddard Center for Astrobiology
FX This work was supported by NASA's Origins of Solar Systems Program and
the Goddard Center for Astrobiology.
NR 50
TC 24
Z9 24
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2012
VL 757
IS 1
AR L11
DI 10.1088/2041-8205/757/1/L11
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 007VQ
UT WOS:000308916900011
ER
PT J
AU Hoffman, JS
Carlson, AE
Winsor, K
Klinkhammer, GP
LeGrande, AN
Andrews, JT
Strasser, JC
AF Hoffman, Jeremy S.
Carlson, Anders E.
Winsor, Kelsey
Klinkhammer, Gary P.
LeGrande, Allegra N.
Andrews, John T.
Strasser, Jeffrey C.
TI Linking the 8.2 ka event and its freshwater forcing in the Labrador Sea
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GLACIAL LAKE AGASSIZ; ABRUPT CLIMATE-CHANGE; SUBPOLAR NORTH-ATLANTIC;
COLD EVENT; HUDSON STRAIT; OUTBURST FLOOD; FINAL DRAINAGE; DEGLACIATION;
TEMPERATURE; CIRCULATION
AB The 8.2 ka event was the last deglacial abrupt climate event. A reduction in the Atlantic meridional overturning circulation (AMOC) attributed to the drainage of glacial Lake Agassiz may have caused the event, but the freshwater signature of Lake Agassiz discharge has yet to be identified in delta O-18 of foraminiferal calcite records from the Labrador Sea, calling into question the connection between freshwater discharge to the North Atlantic and AMOC strength. Using Mg/Ca-paleothermometry, we demonstrate that similar to 3 degrees C of near-surface ocean cooling masked an similar to 1.0 parts per thousand decrease in western Labrador Sea delta O-18 of seawater concurrent with Lake Agassiz drainage. Comparison with North Atlantic delta O-18 of seawater records shows that the freshwater discharge was transported to regions of deep-water formation where it could perturb AMOC and force the 8.2 ka event. Citation: Hoffman, J. S., A. E. Carlson, K. Winsor, G. P. Klinkhammer, A. N. LeGrande, J. T. Andrews, and J. C. Strasser (2012), Linking the 8.2 ka event and its freshwater forcing in the Labrador Sea, Geophys. Res. Lett., 39, L18703, doi:10.1029/2012GL053047.
C1 [Carlson, Anders E.; Winsor, Kelsey] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Hoffman, Jeremy S.; Strasser, Jeffrey C.] Augustana Coll, Dept Geol, Rock Isl, IL 61201 USA.
[Carlson, Anders E.] Univ Wisconsin, Ctr Climat Res, Madison, WI 53706 USA.
[Klinkhammer, Gary P.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Andrews, John T.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Andrews, John T.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
RP Carlson, AE (reprint author), Univ Wisconsin, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA.
EM acarlson@geology.wisc.edu
FU Augustana College Student Summer Research Fellowship; University of
Wisconsin-Madison; National Science Foundation Paleoclimate Program
FX A. Ungerer and S. Marcott assisted with Mg/Ca analyses. A. Mix discussed
methodological approaches. Comments by three reviewers improved this
manuscript. An Augustana College Student Summer Research Fellowship (J.
S. H.), and the University of Wisconsin-Madison and National Science
Foundation Paleoclimate Program (A. E. C.) funded this study. Samples
were provided by the Bedford Institute of Oceanography.
NR 33
TC 24
Z9 24
U1 2
U2 39
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 20
PY 2012
VL 39
AR L18703
DI 10.1029/2012GL053047
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 011AX
UT WOS:000309136800003
ER
PT J
AU Corbett, JG
Su, W
Loeb, NG
AF Corbett, J. G.
Su, W.
Loeb, N. G.
TI Observed effects of sastrugi on CERES top-of-atmosphere clear-sky
reflected shortwave flux over Antarctica
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ENERGY SYSTEM CERES; BIDIRECTIONAL REFLECTANCE; ICE SHEETS; SNOW;
CLOUDS; ALBEDO; TERRA
AB Determining the clear-sky top-of-atmosphere (TOA) albedo over snow from space requires knowledge of the bi-directional reflectance distribution function (BRDF), which itself is strongly influenced by the surface roughness of the snow. Sastrugi, a common element of surface roughness on Antarctica, tend to have a preferred azimuth direction, meaning the BRDF depends on the location and time of sampling. In this study we demonstrate that a sastrugi signal is present in the Clouds and the Earth's Radiant Energy System (CERES) reflectance measurements and TOA albedo estimates, leading to a spurious variation in instantaneous albedo as a function of solar azimuth of up to 0.08. By using the difference in flux between oblique and nadir views, we estimate the biases in monthly-and annual-mean 24-hour energy weighted clear-sky reflected TOA fluxes caused by sastrugi over Antarctica. At the grid box level, statistically significant monthly-mean biases of between +/- 15 Wm(-2) are found. For the entire Antarctic continent, monthly-mean biases are between 0.2 +/- 0.9 Wm(-2) to -1.7 +/- 1.1 Wm(-2) where a negative bias indicates the reflected flux is being underestimated. On an annual basis, the Antarctic bias is between -0.9 +/- 1.1 Wm(-2) and -1.0 +/- 1.1 Wm(-2). For the global annual mean clear-sky TOA flux, the bias caused by the presence of sastrugi is insignificant, -0.01 +/- 0.02 Wm(-2). By examining the anisotropy and the wind direction we infer that the negative TOA flux biases are likely to caused by sastrugi perpendicular to the solar azimuth whereas the positive TOA flux biases are likely to be caused by sastrugi parallel to the solar azimuth.
C1 [Corbett, J. G.] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
[Su, W.; Loeb, N. G.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
RP Corbett, JG (reprint author), NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Mail Stop 420, Hampton, VA 23681 USA.
EM joseph.g.corbett@nasa.gov
NR 22
TC 2
Z9 2
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 20
PY 2012
VL 117
AR D18104
DI 10.1029/2012JD017529
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 011BQ
UT WOS:000309138800001
ER
PT J
AU Poppe, AR
Halekas, JS
Delory, GT
Farrell, WM
AF Poppe, A. R.
Halekas, J. S.
Delory, G. T.
Farrell, W. M.
TI Particle-in-cell simulations of the solar wind interaction with lunar
crustal magnetic anomalies: Magnetic cusp regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LOW-DENSITY PLASMA; ELECTRIC-FIELD; IMPACT BASINS; SURFACE; MOON; SPACE;
PROSPECTOR; MAGNETOMETER; POTENTIALS; MERCURY
AB As the solar wind is incident upon the lunar surface, it will occasionally encounter lunar crustal remanent magnetic fields. These magnetic fields are small-scale, highly non-dipolar, have strengths up to hundreds of nanotesla, and typically interact with the solar wind in a kinetic fashion. Simulations, theoretical analyses, and spacecraft observations have shown that crustal fields can reflect solar wind protons via a combination of magnetic and electrostatic reflection; however, analyses of surface properties have suggested that protons may still access the lunar surface in the cusp regions of crustal magnetic fields. In this first report from a planned series of studies, we use a 1 1/2-dimensional, electrostatic particle-in-cell code to model the self-consistent interaction between the solar wind, the cusp regions of lunar crustal remanent magnetic fields, and the lunar surface. We describe the self-consistent electrostatic environment within crustal cusp regions and discuss the implications of this work for the role that crustal fields may play regulating space weathering of the lunar surface via proton bombardment.
C1 [Poppe, A. R.; Halekas, J. S.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Poppe, A. R.; Halekas, J. S.; Delory, G. T.; Farrell, W. M.] NASA, Lunar Sci Inst, Ames Res Ctr, Mountain View, CA USA.
[Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM poppe@ssl.berkeley.edu
RI Farrell, William/I-4865-2013;
OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128
FU NASA's Lunar Science Institute
FX The authors gratefully acknowledge support from NASA's Lunar Science
Institute. The authors also wish to thank two anonymous reviewers for
constructive comments that greatly improved the manuscript.
NR 83
TC 16
Z9 16
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 20
PY 2012
VL 117
AR A09105
DI 10.1029/2012JA017844
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 011AS
UT WOS:000309136300002
ER
PT J
AU Zenginoglu, A
Galley, CR
AF Zenginoglu, Anil
Galley, Chad R.
TI Caustic echoes from a Schwarzschild black hole
SO PHYSICAL REVIEW D
LA English
DT Article
ID WAVE-PROPAGATION; NORMAL-MODES; PERTURBATIONS; COLLAPSE; SCALAR; TIME
AB We present the first numerical approximation of the scalar Schwarzschild Green function in the time domain, which reveals several universal features of wave propagation in black hole spacetimes. We demonstrate the trapping of energy near the photon sphere and confirm its exponential decay. The trapped wavefront passes through caustics resulting in echoes that propagate to infinity. The arrival times and the decay rate of these caustic echoes are consistent with propagation along null geodesics and the large l limit of quasinormal modes. We show that the fourfold singularity structure of the retarded Green function is due to the well-known action of a Hilbert transform on the trapped wavefront at caustics. A twofold cycle is obtained for degenerate source-observer configurations along the caustic line, where the energy amplification increases with an inverse power of the scale of the source. Finally, we discuss the tail piece of the solution due to propagation within the light cone, up to and including null infinity, and argue that, even with ideal instruments, only a finite number of echoes can be observed. Putting these pieces together, we provide a heuristic expression that approximates the Green function with a few free parameters. Accurate calculations and approximations of the Green function are the most general way of solving for wave propagation in curved spacetimes and should be useful in a variety of studies such as the computation of the self-force on a particle.
C1 [Zenginoglu, Anil; Galley, Chad R.] CALTECH, Pasadena, CA 91125 USA.
[Galley, Chad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zenginoglu, A (reprint author), CALTECH, Pasadena, CA 91125 USA.
OI Zenginoglu, Anil/0000-0001-7896-6268
FU NSF [PHY-1068881]; Sherman Fairchild Foundation; NASA
FX We thank Marc Casals, Sam Dolan, Haixing Miao, Mark Scheel, Bela
Szilagyi, Nicholas Taylor, Dave Tsang, and Huan Yang for discussions. A.
Z. is supported by the NSF Grant No. PHY-1068881, and by a Sherman
Fairchild Foundation Grant to Caltech. CRG is supported by an
appointment to the NASA Postdoctoral Program (administered by Oak Ridge
Associated Universities through a contract with NASA) at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA where part of this research was carried out.
NR 45
TC 15
Z9 15
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD SEP 18
PY 2012
VL 86
IS 6
AR 064030
DI 10.1103/PhysRevD.86.064030
PG 18
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 007EC
UT WOS:000308870600004
ER
PT J
AU Bontognali, TRR
Sessions, AL
Allwood, AC
Fischer, WW
Grotzinger, JP
Summons, RE
Eiler, JM
AF Bontognali, Tomaso R. R.
Sessions, Alex L.
Allwood, Abigail C.
Fischer, Woodward W.
Grotzinger, John P.
Summons, Roger E.
Eiler, John M.
TI Sulfur isotopes of organic matter preserved in 3.45-billion-year-old
stromatolites reveal microbial metabolism
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE early life; biosignature; microbe; paleontology; ion probe
ID MASS-INDEPENDENT FRACTIONATION; GA DRESSER FORMATION; EARLY ARCHEAN ERA;
SULFATE-REDUCTION; WESTERN-AUSTRALIA; PILBARA CRATON; ELEMENTAL SULFUR;
SOUTH-AFRICA; SEDIMENTS; ORIGIN
AB The 3.45-billion-year-old Strelley Pool Formation of Western Australia preserves stromatolites that are considered among the oldest evidence for life on Earth. In places of exceptional preservation, these stromatolites contain laminae rich in organic carbon, interpreted as the fossil remains of ancient microbial mats. To better understand the biogeochemistry of these rocks, we performed microscale in situ sulfur isotope measurements of the preserved organic sulfur, including both Delta S-33 and Delta S-34(CDT). This approach allows us to tie physiological inference from isotope ratios directly to fossil biomass, providing a means to understand sulfur metabolism that is complimentary to, and independent from, inorganic proxies (e.g., pyrite) Delta S-33 values of the kerogen reveal mass-anomalous fractionations expected of the Archean sulfur cycle, whereas Delta S-34(CDT) values show large fractionations at very small spatial scales, including values below -15 parts per thousand. We interpret these isotopic patterns as recording the process of sulfurization of organic matter by H2S in heterogeneous mat pore-waters influenced by respiratory S metabolism. Positive Delta S-33 anomalies suggest that disproportionation of elemental sulfur would have been a prominent microbial process in these communities.
C1 [Bontognali, Tomaso R. R.; Sessions, Alex L.; Fischer, Woodward W.; Grotzinger, John P.; Eiler, John M.] CALTECH, Pasadena, CA 91125 USA.
[Allwood, Abigail C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Summons, Roger E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Bontognali, TRR (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM tb@caltech.edu
OI Bontognali, Tomaso R.R./0000-0003-4917-0388
FU Caltech Center for Microanalysis; Swiss National Science Foundation;
NASA Exobiology program
FX We thank Yunbin Guan for his assistance with the NanoSIMS analyses,
Anthony Carrasquillo for performing the kerogen isolation from the
stromatolites, Arndt Schimmelmann for providing us with the kerogen
standards, Timothy Lyons and Steven Bates for performing the EA-IRMS
measurements, David Mann for preparing the thin sections, and Victoria
Orphan and Stefano Bernasconi for comments and suggestions. This work
was supported by the Caltech Center for Microanalysis, the Swiss
National Science Foundation, and the NASA Exobiology program.
NR 50
TC 36
Z9 37
U1 7
U2 102
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD SEP 18
PY 2012
VL 109
IS 38
BP 15146
EP 15151
DI 10.1073/pnas.1207491109
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 012BS
UT WOS:000309211000024
PM 22949693
ER
PT J
AU Yim, J
Lee, BJ
Kim, C
AF Yim, JinWoo
Lee, Byung Joon
Kim, Chongam
TI Exploring multi-stage shape optimization strategy of multi-body
geometries using Kriging-based model and adjoint method
SO COMPUTERS & FLUIDS
LA English
DT Article
DE Aerodynamic shape optimization; Discrete adjoint method; Kriging model;
Expected Improvement
ID AERODYNAMIC DESIGN OPTIMIZATION; UNSTRUCTURED MESHES; DRAG PREDICTION;
FLOW; FORMULATION; AIRFOIL
AB This paper deals with an efficient and high-fidelity design strategy for wing-body configuration. According to the nature of the design space and the number of design variables, aerodynamic shape optimization is carried out at each design stage by using a selective optimization strategy. In the first stage, global optimization techniques are applied to wing planform design with a few geometric design variables. In the second stage, local optimization techniques are employed to wing surface design with many design variables, which can maintain a sufficient design space with a high Degree of Freedom (DOF) geometric change. For global optimization, the Kriging method in conjunction with a Genetic Algorithm (GA) is used. A searching algorithm exploiting Expected Improvement (EI) design points is introduced to efficiently enhance the quality of the initial Kriging model for the wing planform design. For local optimization, a discrete adjoint method is adopted to obtain sensitivity information by fully hand-differentiating the three-dimensional Euler and N-S equations on an overset mesh topology. By the successive use of the global and local optimization methods, the drag of a multi-body aircraft configuration can be minimized for inviscid and viscous flow conditions while the baseline lift and wing weight are maintained. Throughout the design process, the performances of the test models are improved, compared to those with the single stage design approach. The performance of the proposed multi-stage design framework is evaluated by the drag decomposition method. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Yim, JinWoo; Kim, Chongam] Seoul Natl Univ, Dept Aerosp Engn, Seoul 151742, South Korea.
[Lee, Byung Joon] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Kim, C (reprint author), Seoul Natl Univ, Dept Aerosp Engn, Seoul 151742, South Korea.
EM chongam@snu.ac.kr
FU Korea Science and Engineering Foundation (KOSEF); Korea government
(MEST) [2011-0027486]; NSL (National Space Lab.) program through the
National Research Foundation of Korea under the Ministry of Education,
Science, and Technology [2011-0029871]; KISTI Supercomputing Center
[KSC-2010-C1-0029]; Institute of Advanced Aerospace Technology
FX This work was supported by a Korea Science and Engineering Foundation
(KOSEF) grant funded by the Korea government (MEST) (No. 2011-0027486),
by the NSL (National Space Lab.) program through the National Research
Foundation of Korea under funding from the Ministry of Education,
Science, and Technology (Grant No. 2011-0029871) and by the KISTI
Supercomputing Center (KSC-2010-C1-0029). The authors also appreciate
the financial and administrative help from the Institute of Advanced
Aerospace Technology.
NR 29
TC 2
Z9 3
U1 0
U2 7
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 SEP 15
PY 2012
VL 68
BP 71
EP 87
DI 10.1016/j.compfiuid.2012.07.015
PG 17
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 025KP
UT WOS:000310188100007
ER
PT J
AU Balbin, R
Flexas, MM
Lopez-Jurado, JL
Pena, M
Amores, A
Alemany, F
AF Balbin, R.
Flexas, M. M.
Lopez-Jurado, J. L.
Pena, M.
Amores, A.
Alemany, F.
TI Vertical velocities and biological consequences at a front detected at
the balearic sea
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Ocean circulation; Vertical velocities; Water masses; Plankton
distribution; Western Mediterranean Sea; Balearic Sea
ID WESTERN MEDITERRANEAN-SEA; NORTHERN CURRENT; IBIZA CHANNEL; OCEAN FRONT;
CIRCULATION; VARIABILITY; GULF; CURRENTS; MOTION; COAST
AB An intense oceanic front was detected at the west of Mallorca Island (Balearic sub-basin of the North Western Mediterranean Sea) during an oceanographic survey in December 2009. This contribution analyses the hydrography and geostrophic motions observed at the front, together with the ageostrophic motion derived from the omega equation. The front separated resident Atlantic water (to the north) from more recent Atlantic water (to the south). Maximum upward vertical velocities of 6 m/day were found at the northern side of the front, related with relative maxima of dissolved oxygen and fluorescence. The vertical velocities in this study are mainly due to relative vorticity advection. AVISO altimetry data is used to discuss the advection of the front over a nearby mooring equipped with temperature and salinity sensors at 300 m below the sea surface. The biological implications of the front are discussed by means of acoustic backscatter data. There is an observed increase in mesopelagic fish biomass at the frontal area. Our hypothesis states that the vertical velocities associated to the front would lead to the observed increase in mesopelagic biomass near the front, which is in agreement with previous studies in other frontal systems. (c) 2012 Elsevier Ltd. All rights reserved.
C1 [Balbin, R.; Lopez-Jurado, J. L.; Pena, M.; Alemany, F.] Ctr Oceanog Baleares, Inst Espanol Oceanog, Palma De Mallorca 07015, Spain.
[Flexas, M. M.; Amores, A.] UIB CSIC, Mediterranean Inst Adv Studies, Esporles 07190, Mallorca, Spain.
[Flexas, M. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Balbin, R (reprint author), Ctr Oceanog Baleares, Inst Espanol Oceanog, Muelle de Poniente S-N, Palma De Mallorca 07015, Spain.
EM rosa.balbin@ba.ieo.es
RI Pena, Marian/G-9341-2014; Amores, Angel/H-9535-2015; Balbin,
Rosa/F-8210-2010;
OI Pena, Marian/0000-0002-9000-1060; Amores, Angel/0000-0003-4139-1557;
Balbin, Rosa/0000-0001-5231-1300; Alemany, F.
(Francisco)/0000-0001-6265-5545
FU IDEADOS [CTM2008-04489-C03/MAR]; Spanish Ministry of Science and
Innovation (MICIIN); Regional Government of the Balearic Islands; Jose
Castillejo grant at the Jet Propulsion Laboratory (Pasadena,
California); MICIIN; National Aeronautics and Space Administration;
Consejo Superior de Investigaciones Cientificas (CSIC) within a JAE
Predoctoral scholarship program
FX We appreciate the collaboration of J. Miguel and M. Iglesias for
calibrating the echo sounder, and for their many useful ideas in the
discussion of the results. We would like to thank A. Aparicio and S.
Montserrat, for their help in the data collection, and CTD and mooring
instrument calibration. We wish to thank the IDEADOS Team, for their
help during the survey, and for their comments and suggestions on the
data analysis. We are also obliged to the UTM-CSIC personnel and the
Sarmiento de Gamboa crew for their very professional management of the
cruise. Vertical velocities were calculated with the help of the
publicly available DAToBJETIVO software, developed by D. Gomis at IMEDEA
(UIB-CSIC), and adapted for our particular conditions. The altimeter
products were produced by Ssalto/Duacs and distributed by Aviso, with
support from Cnes (http://www.aviso.oceanobs.com/duacs/). The SST images
has been produced using MyOcean Products (http://www.myocean.eu/).
Chlorophyll-a data is distributed by the OceanColor Web (Feldman and
McClain, 2011). This work is supported by the IDEADOS project
(CTM2008-04489-C03/MAR) funded by the Spanish Ministry of Science and
Innovation (MICIIN). M.M. Flexas acknowledges a postdoctoral fellowship
funded by the Regional Government of the Balearic Islands and a Jose
Castillejo grant at the Jet Propulsion Laboratory (Pasadena, California)
funded by the MICIIN. This research was partially carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. A.
Amores is funded by the Consejo Superior de Investigaciones Cientificas
(CSIC) within a JAE Predoctoral scholarship program.
NR 46
TC 18
Z9 18
U1 1
U2 17
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD SEP 15
PY 2012
VL 47
BP 28
EP 41
DI 10.1016/j.csr.2012.06.008
PG 14
WC Oceanography
SC Oceanography
GA 028DU
UT WOS:000310403800004
ER
PT J
AU Kubar, TL
Waliser, DE
Li, JL
Jiang, XN
AF Kubar, Terence L.
Waliser, Duane E.
Li, J. -L.
Jiang, Xianan
TI On the Annual Cycle, Variability, and Correlations of Oceanic Low-Topped
Clouds with Large-Scale Circulation Using Aqua MODIS and ERA-Interim
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; BOUNDARY-LAYER; TROPICAL PACIFIC; PART I;
MICROPHYSICAL PROPERTIES; STRATOCUMULUS CLOUDS; STATISTICAL-ANALYSES;
STRATUS CLOUDS; OBJECT DATA; SATELLITE
AB Eight years of Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) level-3 cloud data in conjunction with collocated Interim ECMWF Re-Analysis are used to investigate relationships between isolated low-topped cloud fraction (LCF) and dynamics/thermodynamics versus averaging time scale. Correlation coefficients between LCF and -SST exceed 0.70 over 56% of ocean regions from 25 degrees S to 25 degrees N for 90-day running means and exceed 0.70 between LCF and 500-hPa omega (omega(500)) for over one-third of oceans from 50 degrees S to 50 degrees N. Correlations increase most dramatically by increasing the averaging time scale from 1 day to about 15, owing to the large LCF synoptic variability and random effects that are suppressed by averaging. In five regions selected with monthly mean SSTs between 291 and 303 K, SST decreases by -0.13 K %(-1) low-cloud cover increase. Monthly LCF is also correlated with estimated inversion strength (EIS), which is SST dominated in low latitudes and free tropospheric temperature dominated in the northeast Atlantic, Pacific, and midlatitudes, though SST and stability are poor predictors of LCF over the southern oceans.
Where the fraction of variance explained by the annual LCF harmonic is high, maximum LCF tends to lead minimum SST by similar to 15-30 days such that clouds can amplify the SST annual cycle, especially when LCF maxima coexist with insolation minima. Monthly mean LCF tends to scale with omega(500) exponentially over the convective margins and offshore of the Pacific Northwest, but daily climatology relationships indicate that LCF levels off and even diminishes for omega(500) > 0.05 Pa s(-1), suggesting a limit through, perhaps, a too strong suppression of boundary layer heights. This suggests the need for dynamic-regime analysis in diagnosing low cloud/circulation feedbacks.
C1 [Kubar, Terence L.; Waliser, Duane E.; Li, J. -L.; Jiang, Xianan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kubar, TL (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM terry.kubar@jpl.nasa.gov
RI Jiang, Xianan/A-2283-2012
NR 46
TC 17
Z9 17
U1 0
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 SEP 15
PY 2012
VL 25
IS 18
BP 6152
EP 6174
DI 10.1175/JCLI-D-11-00478.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 009PP
UT WOS:000309038000007
ER
PT J
AU Ruzmaikin, A
Aumann, HH
Pagano, TS
AF Ruzmaikin, Alexander
Aumann, Hartmut H.
Pagano, Thomas S.
TI Patterns of CO2 Variability from Global Satellite Data
SO JOURNAL OF CLIMATE
LA English
DT Article
ID ATMOSPHERIC CO2; INTERANNUAL VARIABILITY; TRANSPORT; MISSION; GASES;
MODEL
AB The authors present an analysis of the global midtropospheric CO2 retrieved for all-sky (clear and cloudy) conditions from measurements by the Atmospheric Infrared Radiation Sounder on board the Aqua satellite in 2003-09. The global data coverage allows the identification of the set of CO2 spatial patterns and their time variability by applying principal component analysis and empirical mode decomposition. The first, dominant pattern represents 93% of the variability and exhibits the linear trend of 2 +/- 0.2 ppm yr(-1), as well as annual and interannual dependencies. The single-site record of CO2 at Mauna Loa compares well with variability of this pattern. The first principal component is phase shifted relative to the Southern Oscillation, indicating a causative relationship between the atmospheric CO2 and ENSO. The higher-order patterns show regional details of CO2 distribution and display the semiannual oscillation. The CO2 distributions are compared with the distribution of two major characteristics of air transport: the vertical velocity and potential temperature surfaces at the same height. In agreement with modeling, CO2 concentration closely traces the potential temperature surfaces (isentropes) in middle and high latitudes. However, its vertical transport in the tropics, where these surfaces are mostly horizontal, is suppressed. The results are in agreement with the previous results on annual and interannual CO2 time variability obtained by using the network flask data. This knowledge of the global CO2 spatial patterns can be useful in climate analyses and potentially in the challenging task of connecting CO2 sources and sinks with its distribution in the atmosphere.
C1 [Ruzmaikin, Alexander; Aumann, Hartmut H.; Pagano, Thomas S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alexander.ruzmaikin@jpl.nasa.gov
FU Jet Propulsion Laboratory of the California Institute of Technology;
National Aeronautics and Space Administration
FX This work could not have been done without the support of Mous Chahine,
who initiated and passionately forwarded the retrievals of the AIRS
CO2 data until the last day of his life. We thank Ed Olson,
Steve Licata, and Luc Chen for their help with the AIRS data. We are
grateful to the reviewers for their helpful critical comments. This work
was supported in part by the Jet Propulsion Laboratory of the California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 29
TC 4
Z9 4
U1 0
U2 7
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 SEP 15
PY 2012
VL 25
IS 18
BP 6383
EP 6393
DI 10.1175/JCLI-D-11-00223.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 009PP
UT WOS:000309038000022
ER
PT J
AU Geng, JH
Wang, Q
Luo, T
Case, B
Jiang, SB
Amzajerdian, F
Yu, JR
AF Geng, Jihong
Wang, Qing
Luo, Tao
Case, Bryson
Jiang, Shibin
Amzajerdian, Farzin
Yu, Jirong
TI Single-frequency gain-switched Ho-doped fiber laser
SO OPTICS LETTERS
LA English
DT Article
ID 2 MU-M
AB We demonstrate a single-frequency gain-switched Ho-doped fiber laser based on heavily doped silicate glass fiber fabricated in-house. A Q-switched Tm-doped fiber laser at 1.95 mu m was used to gain-switch the Ho-doped fiber laser via in-band pumping. Output power of the single-frequency gain-switched pulses has been amplified in a cladding-pumped Tm-Ho-codoped fiber amplifier with 1.2 m active fiber pumped at 803 nm. Two different nonlinear effects, i.e., modulation instability and stimulated Brillouin scattering, could be seen in the 10 mu m-core fiber amplifier when the peak power exceeds 3kW. The single-frequency gain-switched fiber laser was operated at 2.05 mu m, a popular laser wavelength for Doppler lidar application. This is the first demonstration of this kind of fiber laser. (C) 2012 Optical Society of America
C1 [Geng, Jihong; Wang, Qing; Luo, Tao; Case, Bryson; Jiang, Shibin] AdValue Photon, Tucson, AZ 85714 USA.
[Amzajerdian, Farzin; Yu, Jirong] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Geng, JH (reprint author), AdValue Photon, 3708 E Columbia St,Suite 100, Tucson, AZ 85714 USA.
EM jgeng@advaluephotonics.com
NR 9
TC 14
Z9 15
U1 2
U2 42
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
EI 1539-4794
J9 OPT LETT
JI Opt. Lett.
PD SEP 15
PY 2012
VL 37
IS 18
BP 3795
EP 3797
PG 3
WC Optics
SC Optics
GA 009SU
UT WOS:000309046300019
PM 23041862
ER
PT J
AU Poppe, AR
Samad, R
Halekas, JS
Sarantos, M
Delory, GT
Farrell, WM
Angelopoulos, V
McFadden, JP
AF Poppe, A. R.
Samad, R.
Halekas, J. S.
Sarantos, M.
Delory, G. T.
Farrell, W. M.
Angelopoulos, V.
McFadden, J. P.
TI ARTEMIS observations of lunar pick-up ions in the terrestrial
magnetotail lobes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LEONID METEOR-SHOWER; SODIUM; ATMOSPHERE; MOON; TAIL
AB We report observations by the twin-probe mission ARTEMIS of pick-up ions of lunar origin obtained during times when the Moon was within the terrestrial magnetotail lobes. These ions were detected as two separate focused beams above the dayside lunar surface. Analysis of these beams has shown that they possess both field-aligned and field-perpendicular velocities, implying the presence of electric fields both parallel and perpendicular to the magnetotail lobe magnetic field. We suggest that the sources of these two electric fields are (a) the near-surface electric field due to the lunar photoelectron sheath and (b) the electric field generated by the magnetotail lobe convection velocity. We use the energy and pitch angle spectra to constrain the source locations and compositions of these ions, and conclude that exospheric ionization of the neutral exosphere is the dominant lunar pick-up ion production mechanism in the tail lobes. Citation: Poppe, A. R., R. Samad, J. S. Halekas, M. Sarantos, G. T. Delory, W. M. Farrell, V. Angelopoulos, and J. P. McFadden (2012), ARTEMIS observations of lunar pick-up ions in the terrestrial magnetotail lobes, Geophys. Res. Lett., 39, L17104, doi:10.1029/2012GL052909.
C1 [Poppe, A. R.; Samad, R.; Halekas, J. S.; Delory, G. T.; McFadden, J. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Poppe, A. R.; Halekas, J. S.; Sarantos, M.; Delory, G. T.; Farrell, W. M.] NASA, Lunar Sci Inst, Ames Res Ctr, Mountain View, CA USA.
[Sarantos, M.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Sarantos, M.; Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Angelopoulos, V.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM poppe@ssl.berkeley.edu
RI Sarantos, Menelaos/H-8136-2013; Farrell, William/I-4865-2013;
OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128
FU NASA's Lunar Science Institute; NASA grant [NAS5-02099]
FX The authors gratefully acknowledge support from NASA's Lunar Science
Institute. The ARTEMIS mission is funded and operated under NASA grant
NAS5-02099. The Kp indices were down-loaded from the NOAA NGDC database.
NR 23
TC 16
Z9 16
U1 2
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 15
PY 2012
VL 39
AR L17104
DI 10.1029/2012GL052909
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 007MK
UT WOS:000308892200006
ER
PT J
AU Nguyen, J
Soibel, A
Rafol, SB
Khoskhlagh, A
Liu, JK
Mumolo, JM
Hoeglund, L
Keo, SA
Ting, DZY
Gunapala, SD
AF Jean Nguyen
Soibel, Alexander
Rafol, Sir B.
Khoskhlagh, Arezou
Liu, John K.
Mumolo, Jason M.
Hoeglund, Linda
Keo, Sam A.
Ting, David Z. -Y.
Gunapala, Sarath D.
TI Inductively Coupled Plasma Etching of Complementary Barrier Infrared
Detector Focal Plane Arrays for Long-Wave Infrared Imaging
SO IEEE PHOTONICS TECHNOLOGY LETTERS
LA English
DT Article
DE Dry etching; focal plane arrays (FPA); long-wave infrared; superlattice
detectors
AB We report on the details of inductively coupled plasma etching for achieving low dark current long-wavelength infrared focal plane arrays (FPAs). External factors that influence the etching process are studied. A high-quality hard mask for excellent pattern transfer is discussed. Next, a suitable mounting technique for good thermal contact is described. Finally, the challenges and differences between etching large 200-mu m test diodes and small 28-mu m FPA pixels are discussed. The complete etching process is then demonstrated on a 320 x 256 complementary barrier infrared detector FPA. The mean dark current density of 2.2 x 10(-4)A/cm(2) is measured at an operating bias of 128 mV with a 50% cutoff wavelength of 8.8 mu m. Good imagery is achieved with an array yielding an 81% fill factor with 97% operability. Operating at T = 80 K, the measured mean noise equivalent differential temperature is 18.6 mK, and the mean detectivity is D* = 1.3 x 10(11) cm-Hz(1/2)/W.
C1 [Jean Nguyen; Soibel, Alexander; Rafol, Sir B.; Khoskhlagh, Arezou; Liu, John K.; Mumolo, Jason M.; Hoeglund, Linda; Keo, Sam A.; Ting, David Z. -Y.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nguyen, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jeannguyen3@gmail.com; alexander.soibel@jpl.nasa.gov;
sir.b.rafol@jpl.nasa.gov; Arezou.Khoshakhlagh@jpl.nasa.gov;
John.k.liu@jpl.nasa.gov; jason.m.mumolo@jpl.nasa.gov;
linda.hoglund@jpl.nasa.gov; Sam.A.Keo@jpl.nasa.gov;
david.z.ting@jpl.nasa.gov; sarath.d.gunapala@jpl.nasa.gov
RI Soibel, Alexander/A-1313-2007
NR 7
TC 2
Z9 2
U1 1
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1041-1135
J9 IEEE PHOTONIC TECH L
JI IEEE Photonics Technol. Lett.
PD SEP 15
PY 2012
VL 24
IS 18
BP 1581
EP 1583
DI 10.1109/LPT.2012.2208949
PG 3
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 000XS
UT WOS:000308424700004
ER
PT J
AU Baranyi, T
Pap, JM
AF Baranyi, Tuende
Pap, Judit M.
TI Active region properties and irradiance variations
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Solar activity; Solar irradiance; Solar variability
ID TOTAL SOLAR IRRADIANCE; SUNSPOTS; VARIABILITY; CYCLE-23; MINIMUM; AREA
AB Total Solar Irradiance (TSI) has been measured for more than three decades. These observations demonstrate that total irradiance changes on time scales ranging from minutes to years and decades. Considerable efforts have been made to understand the physical origin of irradiance variations and to model the observed changes using measures of sunspots and faculae. In this paper, we study the short-term variations in TSI during the declining portion and minimum of solar cycle 22 and the rising portion of cycle 23 (1993-1998). This time interval of low solar activity allows us to study the effect of individual sunspot groups on TSI in detail. In this paper, we indicate that the effect of sunspot groups on total irradiance may depend on their type in the Zurich classification system and/or their evolution, and on their magnetic configuration. Some uncertainties in the data and other effects are also discussed. (c) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Baranyi, Tuende] Hungarian Acad Sci, Heliophys Observ, H-4010 Debrecen, Hungary.
[Pap, Judit M.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Baranyi, T (reprint author), Hungarian Acad Sci, Heliophys Observ, POB 30, H-4010 Debrecen, Hungary.
EM baranyi@tigris.unideb.hu; judit.m.pap@nasa.gov
FU ESA PECS project [C98081]; NASA Grant [NNX09AB83G]; Living With a Star
Program
FX This work was supported by the ESA PECS project No. C98081 (T.B.) and by
NASA Grant NNX09AB83G, supported by the Living With a Star Program
(J.P.).
NR 27
TC 0
Z9 0
U1 0
U2 2
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD SEP 15
PY 2012
VL 50
IS 6
BP 676
EP 682
DI 10.1016/j.asr.2011.11.037
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 991FU
UT WOS:000307687700005
ER
PT J
AU da Silva, JC
Saxena, A
Balaban, E
Goebel, K
AF da Silva, Jonny Carlos
Saxena, Abhinav
Balaban, Edward
Goebel, Kai
TI A knowledge-based system approach for sensor fault modeling, detection
and mitigation
SO EXPERT SYSTEMS WITH APPLICATIONS
LA English
DT Article
DE Detection; Sensor failure; Expert system; Neural Network
ID PROTOTYPE; DIAGNOSIS
AB Sensors are vital components for control and advanced health management techniques. However, sensors continue to be considered the weak link in many engineering applications since often they are less reliable than the system they are observing. This is in part due to the sensors' operating principles and their susceptibility to interference from the environment. Detecting and mitigating sensor failure modes are becoming increasingly important in more complex and safety-critical applications. This paper reports on different techniques for sensor fault detection, disambiguation, and mitigation. It presents an expert system that uses a combination of object-oriented modeling, rules, and semantic networks to deal with the most common sensor faults, such as bias, drift, scaling, and dropout, as well as system faults. The paper also describes a sensor correction module that is based on fault parameters extraction (for bias, drift, and scaling fault modes) as well as utilizing partial redundancy for dropout sensor fault modes). The knowledge-based system was derived from the results obtained in a previously deployed Neural Network (NN) application for fault detection and disambiguation. Results are illustrated on an electromechanical actuator application where the system faults are jam and spalling. In addition to the functions implemented in the previous work, system fault detection under sensor failure was also modeled. The paper includes a sensitivity analysis that compares the results previously obtained with the NN. It concludes with a discussion of similarities and differences between the two approaches and how the knowledge based system provides additional functionality compared to the NN implementation. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [da Silva, Jonny Carlos; Saxena, Abhinav] NASA, SGT Inc, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
[da Silva, Jonny Carlos] Univ Fed Santa Catarina, Dept Mech Engn, BR-88040900 Florianopolis, SC, Brazil.
RP da Silva, JC (reprint author), NASA, SGT Inc, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
EM jonny@emc.ufsc.br; abhinav.saxena@nasa.gov; edward.balaban@nasa.gov;
kai.goebel@nasa.gov
FU CAPES Foundation, Brazil [4095/10-3]; UFSC - Federal University of Santa
Catarina (Brazil); NASA Ames Research Center
FX This project was developed under Grant 4095/10-3, CAPES Foundation,
Brazil. The authors would also like to thank UFSC - Federal University
of Santa Catarina (Brazil), and NASA Ames Research Center for their
support in this project.
NR 17
TC 13
Z9 13
U1 1
U2 26
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0957-4174
J9 EXPERT SYST APPL
JI Expert Syst. Appl.
PD SEP 15
PY 2012
VL 39
IS 12
BP 10977
EP 10989
DI 10.1016/j.eswa.2012.03.026
PG 13
WC Computer Science, Artificial Intelligence; Engineering, Electrical &
Electronic; Operations Research & Management Science
SC Computer Science; Engineering; Operations Research & Management Science
GA 966UQ
UT WOS:000305863300066
ER
PT J
AU Kort, EA
Frankenberg, C
Miller, CE
Oda, T
AF Kort, Eric A.
Frankenberg, Christian
Miller, Charles E.
Oda, Tom
TI Space-based observations of megacity carbon dioxide
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GREENHOUSE-GAS EMISSIONS; PART 1; CO2; VALIDATION; URBAN
AB Urban areas now house more than half the world's population, and are estimated to contribute over 70% of global energy-related CO2 emissions. Many cities have emission reduction policies in place, but lack objective, observationbased methods for verifying their outcomes. Here we demonstrate the potential of satellite-borne instruments to provide accurate global monitoring of megacity CO2 emissions using GOSAT observations of column averaged CO2 dry air mole fraction (X-CO2) collected over Los Angeles and Mumbai. By differencing observations over the megacity with those in nearby background, we observe robust, statistically significant X-CO2 enhancements of 3.2 +/- 1.5 ppm for Los Angeles and 2.4 +/- 1.2 ppm for Mumbai, and find these enhancements can be exploited to track anthropogenic emission trends over time. We estimate that X-CO2 changes as small as 0.7 ppm in Los Angeles, corresponding to a 22% change in emissions, could be detected with GOSAT at the 95% confidence level. Citation: Kort, E. A., C. Frankenberg, C. E. Miller, and T. Oda (2012), Space-based observations of megacity carbon dioxide, Geophys. Res. Lett., 39, L17806, doi:10.1029/2012GL052738.
C1 [Kort, Eric A.] CALTECH, WM Keck Inst Space Studies, Pasadena, CA 91125 USA.
[Kort, Eric A.; Frankenberg, Christian; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Oda, Tom] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Oda, Tom] NOAA, Earth Syst Res Lab, Boulder, CO USA.
RP Kort, EA (reprint author), CALTECH, WM Keck Inst Space Studies, Pasadena, CA 91125 USA.
EM eric.a.kort@jpl.nasa.gov
RI Kort, Eric/F-9942-2012; Frankenberg, Christian/A-2944-2013
OI Kort, Eric/0000-0003-4940-7541; Frankenberg,
Christian/0000-0002-0546-5857
FU W. M. Keck Institute for Space Studies
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. EAK thanks the W. M.
Keck Institute for Space Studies for support. GOSAT Level 1B products
(spectral data) were provided by the GOSAT Project (JAXA, NIES, and
Ministry of the Environment Japan) through its collaboration with NASA's
Atmospheric CO2 Observations from Spaces (ACOS) team. The
XCO2 data used in this work were processed by the ACOS team
using software build 2.9. The authors thank the GOSAT and OCO/ACOS teams
for continued collaboration and detailed technical discussions. The
authors wish to thank Paul Wennberg, Yuk Yung, Michael Gunson, and
Annmarie Eldering for insightful and constructive suggestions and
comments.
NR 25
TC 47
Z9 47
U1 0
U2 42
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 14
PY 2012
VL 39
AR L17806
DI 10.1029/2012GL052738
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 007MF
UT WOS:000308891700004
ER
PT J
AU Kanakidou, M
Duce, RA
Prospero, JM
Baker, AR
Benitez-Nelson, C
Dentener, FJ
Hunter, KA
Liss, PS
Mahowald, N
Okin, GS
Sarin, M
Tsigaridis, K
Uematsu, M
Zamora, LM
Zhu, T
AF Kanakidou, Maria
Duce, Robert A.
Prospero, Joseph M.
Baker, Alex R.
Benitez-Nelson, Claudia
Dentener, Frank J.
Hunter, Keith A.
Liss, Peter S.
Mahowald, Natalie
Okin, Gregory S.
Sarin, Manmohan
Tsigaridis, Kostas
Uematsu, Mitsuo
Zamora, Lauren M.
Zhu, Tong
TI Atmospheric fluxes of organic N and P to the global ocean
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
ID MASS-SPECTROMETRY; NITROGEN DEPOSITION; PHOSPHORUS CYCLE;
NORTH-ATLANTIC; AEROSOL; SECONDARY; TROPOSPHERE; CARBON; EMISSIONS;
AEROCOM
AB The global tropospheric budget of gaseous and particulate non-methane organic matter (OM) is re-examined to provide a holistic view of the role that OM plays in transporting the essential nutrients nitrogen and phosphorus to the ocean. A global 3-dimensional chemistry-transport model was used to construct the first global picture of atmospheric transport and deposition of the organic nitrogen (ON) and organic phosphorus (OP) that are associated with OM, focusing on the soluble fractions of these nutrients. Model simulations agree with observations within an order of magnitude. Depending on location, the observed water soluble ON fraction ranges from similar to 3% to 90% (median of similar to 35%) of total soluble N in rainwater; soluble OP ranges from similar to 20-83% (median of similar to 35%) of total soluble phosphorus. The simulations suggest that the global ON cycle has a strong anthropogenic component with similar to 45% of the overall atmospheric source (primary and secondary) associated with anthropogenic activities. In contrast, only 10% of atmospheric OP is emitted from human activities. The model-derived present-day soluble ON and OP deposition to the global ocean is estimated to be similar to 16 Tg-N/yr and similar to 0.35 Tg-P/yr respectively with an order of magnitude uncertainty. Of these amounts similar to 40% and similar to 6%, respectively, are associated with anthropogenic activities, and 33% and 90% are recycled oceanic materials. Therefore, anthropogenic emissions are having a greater impact on the ON cycle than the OP cycle; consequently increasing emissions may increase P-limitation in the oligotrophic regions of the world's ocean that rely on atmospheric deposition as an important nutrient source.
C1 [Kanakidou, Maria] Univ Crete, Dept Chem, Environm Chem Proc Lab, GR-71003 Iraklion, Greece.
[Duce, Robert A.] Texas A&M Univ, Dept Oceanog, College Stn, TX 77843 USA.
[Duce, Robert A.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
[Prospero, Joseph M.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Baker, Alex R.; Liss, Peter S.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Benitez-Nelson, Claudia] Univ S Carolina, Dept Earth & Ocean Sci, Columbia, SC 29208 USA.
[Benitez-Nelson, Claudia] Univ S Carolina, Marine Sci Program, Columbia, SC 29208 USA.
[Dentener, Frank J.] Inst Environm & Sustainabil, Joint Res Ctr, European Commiss, Ispra, Italy.
[Hunter, Keith A.] Univ Otago, Div Sci, Dunedin, New Zealand.
[Mahowald, Natalie] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY USA.
[Okin, Gregory S.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
[Sarin, Manmohan] Phys Res Lab, Dept Geosci, Ahmadabad 380009, Gujarat, India.
[Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Tsigaridis, Kostas] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA.
[Uematsu, Mitsuo] Univ Tokyo, Ocean Res Inst, Tokyo 164, Japan.
[Zamora, Lauren M.] Helmholtz Ctr Ocean Res Kiel, GEOMAR, Kiel, Germany.
[Zhu, Tong] Peking Univ, Coll Environm Sci & Engn, Beijing 100871, Peoples R China.
RP Kanakidou, M (reprint author), Univ Crete, Dept Chem, Environm Chem Proc Lab, POB 2208, GR-71003 Iraklion, Greece.
EM mariak@chemistry.uoc.gr
RI Baker, Alex/D-1233-2011; Tsigaridis, Kostas/K-8292-2012; LISS,
Peter/A-8219-2013; Duce, Robert/A-9917-2010; Mahowald,
Natalie/D-8388-2013; Zamora, Lauren/E-6972-2011; ZHU, TONG/H-6501-2011;
Kanakidou, Maria/D-7882-2012;
OI Okin, Gregory/0000-0002-0484-3537; Baker, Alex/0000-0002-8365-8953;
Tsigaridis, Kostas/0000-0001-5328-819X; Mahowald,
Natalie/0000-0002-2873-997X; Zamora, Lauren/0000-0002-0878-4378;
Benitez-Nelson, Claudia/0000-0002-1004-5048; Kanakidou,
Maria/0000-0002-1724-9692; Prospero, Joseph/0000-0003-3608-6160
FU Global Atmosphere Watch (GAW); World Weather Research Programme (WWRP)
of the World Meteorological Organization (WMO); International Maritime
Organization (IMO); ICSU Scientific Committee on Oceanic Research
(SCOR); Swedish International Development Agency (SIDA); University of
Arizona; European Commission Joint Research Centre; University of Crete,
Greece
FX This paper resulted from the deliberations of GESAMP Working Group 38,
The Atmospheric Input of Chemicals to the Ocean. We thank the Global
Atmosphere Watch (GAW) and the World Weather Research Programme (WWRP)
of the World Meteorological Organization (WMO), the International
Maritime Organization (IMO), the ICSU Scientific Committee on Oceanic
Research (SCOR), the Swedish International Development Agency (SIDA),
the University of Arizona, and the European Commission Joint Research
Centre for support of this work. M.K. acknowledges support from the
University of Crete, Greece. We thank K. Kawamura for fruitful
discussions and J. van Aardenne and U. Doering for the anthropogenic
emission global inventories. Technical support for the TM4-ECPL model
emission updates by N. Daskalakis and S. Myriokefalitakis is
acknowledged.
NR 81
TC 53
Z9 54
U1 4
U2 108
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 SEP 14
PY 2012
VL 26
AR GB3026
DI 10.1029/2011GB004277
PG 12
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA 007MX
UT WOS:000308893500002
ER
PT J
AU Yang, MYM
Vay, SA
Stohl, A
Choi, Y
Diskin, GS
Sachse, GW
Blake, DR
AF Yang, Mei Ying Melissa
Vay, Stephanie A.
Stohl, Andreas
Choi, Yonghoon
Diskin, Glenn S.
Sachse, Glen W.
Blake, Donald R.
TI Chemical composition of tropospheric air masses encountered during high
altitude flights (11.5 km) during the 2009 fall Operation Ice Bridge
field campaign
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TRACE GASES; STRATOSPHERE; PACIFIC
AB As part of the 2009 Operation Ice Bridge campaign, the NASA DC-8 aircraft was used to fill the data-time gap in laser observation of the changes in ice sheets, glaciers and sea ice between ICESat-I (Ice, Cloud, and land Elevation Satellite) and ICESat-II. Complementing the cryospheric instrument payload were four in situ atmospheric sampling instruments integrated onboard to measure trace gas concentrations of CO2, CO, N2O, CH4, water vapor and various VOCs (Volatile Organic Compounds). This paper examines two plumes encountered at high altitude (12 km) during the campaign; one during a southbound transit flight (13 degrees S) and the other at 86 degrees S over Antarctica. The data presented are especially significant as the Southern Hemisphere is heavily under-sampled during the austral spring, with few if any high-resolution airborne observations of atmospheric gases made over Antarctica. Strong enhancements of CO, CH4, N2O, CHCl3, OCS, C2H6, C2H2 and C3H8 were observed in the two intercepted air masses that exhibited variations in VOC composition suggesting different sources. The transport model FLEXPART showed that the 13 degrees S plume contained predominately biomass burning emissions originating from Southeast Asia and South Africa, while both anthropogenic and biomass burning emissions were observed at 86 degrees S with South America and South Africa as indicated source regions. The data presented here show evidence that boundary layer pollution is transported from lower latitudes toward the upper troposphere above the South Pole, which may not have been observed in the past.
C1 [Yang, Mei Ying Melissa; Vay, Stephanie A.; Choi, Yonghoon; Diskin, Glenn S.; Sachse, Glen W.] NASA, Chem & Dynam Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Stohl, Andreas] Norwegian Inst Air Res, Kjeller, Norway.
[Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA.
[Choi, Yonghoon; Sachse, Glen W.] Natl Inst Aerosp, Hampton, VA USA.
RP Yang, MYM (reprint author), NASA, Chem & Dynam Branch, Langley Res Ctr, MS 483, Hampton, VA 23681 USA.
EM melissa.yang@nasa.gov
RI Stohl, Andreas/A-7535-2008
OI Stohl, Andreas/0000-0002-2524-5755
FU NASA; Norwegian Research Council
FX Research for the project was funded by NASA's Upper Atmosphere Research
Program (UARP). A.S. was supported by the Norwegian Research Council in
the framework of the CLIMSLIP project. Special thanks to the OIB Science
Team, the DACOM/DLH research group, AVOCET research group, and the UCI
Blake research group. Special thanks to the reviewers from Journal of
Geophysical Research in helping to further refine and improve our paper.
NR 23
TC 1
Z9 1
U1 1
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 14
PY 2012
VL 117
AR D17306
DI 10.1029/2012JD017858
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 007MQ
UT WOS:000308892800001
ER
PT J
AU Keith, DJ
Milstead, B
Walker, H
Snook, H
Szykman, J
Wusk, M
Kagey, L
Howell, C
Mellanson, C
Drueke, C
AF Keith, Darryl J.
Milstead, Bryan
Walker, Henry
Snook, Hilary
Szykman, James
Wusk, Michael
Kagey, Les
Howell, Charles
Mellanson, Cecil
Drueke, Christopher
TI Trophic status, ecological condition, and cyanobacteria risk of New
England lakes and ponds based on aircraft remote sensing
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE aircraft remote sensing; chlorophyll a; cyanobacteria; New England lakes
and ponds
ID TURBID PRODUCTIVE WATERS; CHLOROPHYLL-A; SEMIANALYTICAL MODEL; INLAND
WATERS; REFLECTANCE; QUALITY; RETRIEVAL; BLOOMS
AB Aircraft remote sensing of freshwater ecosystems offers federal and state monitoring agencies an ability to meet their assessment requirements by rapidly acquiring information on ecosystem responses to environmental change for water bodies that are below the resolution of space-based platforms. During this study, hyperspectral data were collected over a two-day period from glacial lakes, ponds, and man-made reservoirs in New Hampshire, Massachusetts, Connecticut, and Rhode Island. These lakes ranged from five to greater than 1600 hectares and oligotrophic-mesotrophic to eutrophic and hypereutrophic conditions. Water samples were collected by several New England state agencies coincident with the airborne remote-sensing flights to provide ground reference data for algorithm development and testing. Using an inverse modeling approach remotely sensed reflectances from the near-infrared to red portion of the spectrum were used to develop an empirical model to estimate chlorophyll a concentrations. The accuracy of the algorithm was assessed from the RSM error of predicted and measured chlorophyll values for all lakes sampled. Results showed a strong statistical relationship between measured and predicted values. The predicted chlorophyll concentrations were used to assess the biological condition, trophic status, and recreational risk to human health for the New England lakes and ponds surveyed. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.JRS.6.063577]
C1 [Keith, Darryl J.; Milstead, Bryan; Walker, Henry] US EPA, Natl Hlth & Environm Effects Lab, Atlantic Ecol Div, Narragansett, RI 02882 USA.
[Snook, Hilary] US EPA, EPA Reg 1, New England Reg Lab, Chelmsford, MA 01863 USA.
[Szykman, James] US EPA, Natl Exposure Res Lab, Environm Serv Div, Res Triangle Pk, NC 27709 USA.
[Wusk, Michael; Kagey, Les; Howell, Charles; Mellanson, Cecil] NASA, Langley Aerosp Res Ctr, Div Res Serv, Hampton, VA 23681 USA.
[Drueke, Christopher] NASA, Langley Aerosp Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23681 USA.
RP Keith, DJ (reprint author), US EPA, Natl Hlth & Environm Effects Lab, Atlantic Ecol Div, Narragansett, RI 02882 USA.
EM keith.darryl@epa.gov
FU US Environmental Protection Agency through the Remote Sensing and Flight
Services
FX Although the research described in this article has been funded wholly
by the US Environmental Protection Agency through the Remote Sensing and
Flight Services Support for USEPA's Air and Ecological Research Program
cooperative agreement to NASA, it has not been subjected to agency
review. Therefore it does not necessarily reflect the views of the
agency. This is contribution number ORD 1659 of the Atlantic Ecology
Division, National Health and Environmental Effects Research Laboratory,
Office of Research and Development, US Environmental Protection Agency.
Any mention of trade names or commercial products does not constitute
endorsement or recommendation for use.
NR 49
TC 3
Z9 3
U1 0
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 SEP 13
PY 2012
VL 6
AR 063577
DI 10.1117/1.JRS.6.063577
PG 22
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 032FG
UT WOS:000310697600001
ER
PT J
AU Li, YF
Qian, H
Wang, Y
Cucinotta, FA
AF Li, Yongfeng
Qian, Hong
Wang, Ya
Cucinotta, Francis A.
TI A Stochastic Model of DNA Fragments Rejoining
SO PLOS ONE
LA English
DT Article
ID DOUBLE-STRAND BREAKS; INDUCE CHROMOSOME BREAKAGE; ENERGY-TRANSFER
RADIATION; IONIZING-RADIATION; SPACE EXPLORATION; GAMMA-H2AX FOCI;
HUMAN-CELLS; DSB-REPAIR; END; KU
AB When cells are exposed to ionizing radiation, DNA damages in the form of single strand breaks (SSBs), double strand breaks (DSBs), base damage or their combinations are frequent events. It is known that the complexity and severity of DNA damage depends on the quality of radiation, and the microscopic dose deposited in small segments of DNA, which is often related to the linear transfer energy (LET) of the radiation. Experimental studies have suggested that under the same dose, high LET radiation induces more small DNA fragments than low-LET radiation, which affects Ku efficiently binding with DNA end and might be a main reason for high-LET radiation induced RBE [1] since DNA DSB is a major cause for radiationinduced cell death. In this work, we proposed a mathematical model of DNA fragments rejoining according to nonhomologous end joining (NHEJ) mechanism. By conducting Gillespie's stochastic simulation, we found several factors that impact the efficiency of DNA fragments rejoining. Our results demonstrated that aberrant DNA damage repair can result predominantly from the occurrence of a spatial distribution of DSBs leading to short DNA fragments. Because of the low efficiency that short DNA fragments recruit repair protein and release the protein residue after fragments rejoining, Kudependent NHEJ is significantly interfered with short fragments. Overall, our work suggests that inhibiting the Kudependent NHEJ may significantly contribute to the increased efficiency for cell death and mutation observed for high LET radiation.
C1 [Li, Yongfeng] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
[Qian, Hong] Univ Washington, Dept Appl Math, Seattle, WA 98195 USA.
[Wang, Ya] Emory Univ, Dept Radiat Oncol, Atlanta, GA 30322 USA.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Li, YF (reprint author), Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
EM francis.a.cucinotta@nasa.gov
FU NASA Space Radiation Program
FX This work was supported by the NASA Space Radiation Program. The funders
had no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 44
TC 15
Z9 15
U1 0
U2 6
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 SEP 13
PY 2012
VL 7
IS 9
AR e44293
DI 10.1371/journal.pone.0044293
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 005ZK
UT WOS:000308788700018
PM 23028515
ER
PT J
AU Koch, GJ
Beyon, JY
Modlin, EA
Petzar, PJ
Woll, S
Petros, M
Yu, JR
Kavaya, MJ
AF Koch, Grady J.
Beyon, Jeffrey Y.
Modlin, Edward A.
Petzar, Paul J.
Woll, Steve
Petros, Mulugeta
Yu, Jirong
Kavaya, Michael J.
TI Side-scan Doppler lidar for offshore wind energy applications
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE wind; lidar; lasers; meteorology
ID TURBINE
AB A field demonstration was done from Virginia Beach, Virginia, to show the use of high-energy (250-mJ) eyesafe Doppler lidar for measurements of offshore wind. The lidar is located onshore and pointed near-horizontally to reach a target area many kilometers away. In sample measurements, the lidar scan's hypothetical turbine is located 6 km away. For one beam elevation of interest, the horizontal wind vector is measured by scanning the beam in azimuth. The elevation can then be changed to profile the wind at many altitudes. An example measurement is shown in which wind vector is determined at six altitudes covering the height of a supposed turbine and above. In addition to the wind vector, wind shear is measured across a turbine blade span width. Over a two-week period in October 2011, range capability was found to vary from 4.5 to 17 km depending on weather and aerosol backscatter conditions. A comparison was made with an anemometer to validate the lidar's measurements. (c) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.JRS.6.063562]
C1 [Koch, Grady J.; Beyon, Jeffrey Y.; Modlin, Edward A.; Petzar, Paul J.; Petros, Mulugeta; Yu, Jirong; Kavaya, Michael J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Woll, Steve] WeatherFlow Inc, Poquoson, VA 23662 USA.
RP Koch, GJ (reprint author), NASA, Langley Res Ctr, Mail Stop 468, Hampton, VA 23681 USA.
EM grady.j.koch@nasa.gov
FU NASA Earth Science Technology Office
FX Development of the lidar instrument and this field measurement were
funded by the NASA Earth Science Technology Office. Thanks are owed to
Heather Lawrence, Spencer Layne, and Captain Charles Stuppard for
hosting the lidar at the Joint Expeditionary Base Little Creek-Fort
Story. George Hagerman of the Virginia Coastal Energy Research
Consortium provided input on the measurement needs and goals for
offshore wind.
NR 11
TC 7
Z9 7
U1 0
U2 16
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 SEP 12
PY 2012
VL 6
AR 063562
DI 10.1117/1.JRS.6.063562
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 032DK
UT WOS:000310692100002
ER
PT J
AU Numata, K
Riris, H
Li, S
Wu, S
Kawa, SR
Krainak, M
Abshire, J
AF Numata, Kenji
Riris, Haris
Li, Steve
Wu, Stewart
Kawa, Stephan R.
Krainak, Michael
Abshire, James
TI Ground demonstration of trace gas lidar based on optical parametric
amplifier
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE optical parametric amplifier; lidar; differential absorption lidar;
space instrumentation
ID POLED LITHIUM-NIOBATE; DIFFERENTIAL ABSORPTION LIDAR; OSCILLATOR;
GENERATOR; METHANE; PROFILE; SYSTEM; CH4; CO2
AB We report on the development effort of a nanosecond-pulsed optical parametric amplifier (OPA) for remote trace gas measurements for Mars and Earth. The OPA output has similar to 500 MHz linewidth and is widely tunable at both near-infrared and mid-infrared wavelengths, with an optical-optical conversion efficiency of up to similar to 39%. Using this laser source, we demonstrated open-path measurements of CH4 (3291 and 1652 nm), CO2 (1573 nm), H2O (1652 nm), and CO (4764 nm) on the ground. The simplicity, tunability, and power scalability of the OPA make it a strong candidate for general planetary lidar instruments, which will offer important information on the origins of the planet's geology, atmosphere, and potential for biology. (c) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.JRS.6.063561]
C1 [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Numata, Kenji; Riris, Haris; Li, Steve; Wu, Stewart; Kawa, Stephan R.; Krainak, Michael; Abshire, James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Numata, K (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM kenji.numata@nasa.gov
RI Riris, Haris/D-1004-2013; Kawa, Stephan/E-9040-2012; Abshire,
James/I-2800-2013
FU NASA Astrobiology Program's Astrobiology Science and Technology
Instrument Development (ASTID) Program
FX This work is supported by the NASA Astrobiology Program's Astrobiology
Science and Technology Instrument Development (ASTID) Program.
NR 22
TC 8
Z9 9
U1 2
U2 27
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 SEP 12
PY 2012
VL 6
AR 063561
DI 10.1117/1.JRS.6.063561
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 032DK
UT WOS:000310692100001
ER
PT J
AU Anderson, JD
Morris, JR
AF Anderson, John D.
Morris, J. R.
TI Brans-Dicke theory and the Pioneer anomaly
SO PHYSICAL REVIEW D
LA English
DT Article
ID GENERAL-RELATIVITY; MACHS PRINCIPLE
AB Scalar-tensor theory offers the possibility of a modification of Newtonian gravity due to the presence of a 4d scalar dilaton field. The prototypical version of such a theory, massless Brans-Dicke theory, is considered here in the Einstein frame representation. The acceleration of a test mass is obtained from the exact 4d Xanthopoulos-Zannias solutions with spherical symmetry. The deviation of this acceleration from the pure Newtonian gravitational acceleration is examined to see if it can account for the anomalous Pioneer acceleration, while satisfying solar system constraints. Theoretical considerations, along with limits inferred from Pioneer 10 data, suggest that Brans-Dicke gravity could account for no more than a small fraction of the Pioneer anomaly, so that a complete explanation of the anomaly must lie elsewhere.
C1 [Morris, J. R.] Indiana Univ NW, Dept Phys, Gary, IN 46408 USA.
[Anderson, John D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM jdandy@earthlink.net; jmorris@iun.edu
NR 21
TC 6
Z9 6
U1 0
U2 3
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 SEP 12
PY 2012
VL 86
IS 6
AR 064023
DI 10.1103/PhysRevD.86.064023
PG 5
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 003WO
UT WOS:000308642300006
ER
PT J
AU Dombrowski, MP
LaBelle, J
Rowland, DE
Pfaff, RF
Kletzing, CA
AF Dombrowski, M. P.
LaBelle, J.
Rowland, D. E.
Pfaff, R. F.
Kletzing, C. A.
TI Interpretation of vector electric field measurements of bursty Langmuir
waves in the cusp
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID AURORAL IONOSPHERE; ROCKET OBSERVATIONS; HYBRID WAVES; FREJA;
TURBULENCE; FREQUENCY; SCIFER; PLASMA; HISS
AB An analysis of auroral Langmuir waves in the cusp observed by two high-frequency electric field instruments on the TRICE high-flyer sounding rocket shows many examples of Langmuir wave bursts modulated at approximately 10 kHz. Previous studies have explained these and similar observations as the result of beating between waves with very close frequencies near the Langmuir cutoff, resulting from either wave-wave interactions or independent linear excitations. The unique three-dimensional (3-D) data set provided by the NASA Goddard Space Flight Center TAEFWD instrument shows that up to 25% of waveforms selected from the most intense bursts exhibit anisotropic modulations, i.e., the beat nulls and peaks are not aligned in time across the three perpendicular electric field components. Modulations of this type arise when superposed wave normal modes possess differing polarizations, and simulations using wave modes calculated with the J-WHAMP numerical dispersion code show (1) that waves with differing polarizations can exist in conditions like those observed by TRICE-High and (2) that superpositions of such waves can produce anisotropic modulation. Fourier analysis of the 3-D waveform data suggests that both linear and elliptically polarized waves are present near the Langmuir cutoff at these times. These observations illustrate how 3-D measurements can give valuable insight into the nature of wave interactions in the auroral plasma environment.
C1 [Dombrowski, M. P.; LaBelle, J.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Rowland, D. E.; Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
RP Dombrowski, MP (reprint author), Dartmouth Coll, Dept Phys & Astron, Rm 315,6127 Wilder Lab, Hanover, NH 03755 USA.
EM mpd@dartmouth.edu
RI Rowland, Douglas/F-5589-2012; Pfaff, Robert/F-5703-2012
OI Rowland, Douglas/0000-0003-0948-6257; Kletzing,
Craig/0000-0002-4136-3348; Pfaff, Robert/0000-0002-4881-9715
FU NASA [NNG04WC24G, NNX12AI44G, NNX10AL81H]
FX This study was supported by NASA grants NNG04WC24G, NNX12AI44G, and
NNX10AL81H.
NR 22
TC 0
Z9 0
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 12
PY 2012
VL 117
AR A09209
DI 10.1029/2012JA017741
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 007LF
UT WOS:000308889100002
ER
PT J
AU Hansen, J
Sato, M
Ruedy, R
AF Hansen, James
Sato, Makiko
Ruedy, Reto
TI Perception of climate change
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE climate impacts; climate anomalies; heat waves
ID SURFACE-TEMPERATURE ANALYSIS; SEA-LEVEL CHANGE; AMPLIFICATION; DROUGHT
AB "Climate dice," describing the chance of unusually warm or cool seasons, have become more and more "loaded" in the past 30 y, coincident with rapid global warming. The distribution of seasonal mean temperature anomalies has shifted toward higher temperatures and the range of anomalies has increased. An important change is the emergence of a category of summertime extremely hot outliers, more than three standard deviations (3 sigma) warmer than the climatology of the 1951-1980 base period. This hot extreme, which covered much less than 1% of Earth's surface during the base period, now typically covers about 10% of the land area. It follows that we can state, with a high degree of confidence, that extreme anomalies such as those in Texas and Oklahoma in 2011 and Moscow in 2010 were a consequence of global warming because their likelihood in the absence of global warming was exceedingly small. We discuss practical implications of this substantial, growing, climate change.
C1 [Hansen, James; Sato, Makiko] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hansen, James; Sato, Makiko] Columbia Univ, Earth Inst, New York, NY 10025 USA.
[Ruedy, Reto] Trinnovim Ltd Liabil Co, New York, NY 10025 USA.
RP Hansen, J (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM james.e.hansen@nasa.gov
RI Langholtz, Matthew/B-9416-2012
OI Langholtz, Matthew/0000-0002-8153-7154
FU ClimateWorks
FX We thank Tom Karl, Andrew Weaver, and an anonymous editor for helpful
reviews that significantly improved the paper, Gerry Lenfest (Lenfest
Foundation), Lee Wasserman (Rockefeller Family Foundation), Stephen
Toben (Flora Family Foundation), NASA program managers Jack Kaye and
David Considine and ClimateWorks for research support.
NR 33
TC 351
Z9 366
U1 41
U2 289
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD SEP 11
PY 2012
VL 109
IS 37
BP E2415
EP E2423
DI 10.1073/pnas.1205276109
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 012AP
UT WOS:000309208000005
PM 22869707
ER
PT J
AU Priester, JH
Ge, Y
Mielke, RE
Horst, AM
Moritz, SC
Espinosa, K
Gelb, J
Walker, SL
Nisbet, RM
An, YJ
Schimel, JP
Palmer, RG
Hernandez-Viezcas, JA
Zhao, LJ
Gardea-Torresdey, JL
Holden, PA
AF Priester, John H.
Ge, Yuan
Mielke, Randall E.
Horst, Allison M.
Moritz, Shelly Cole
Espinosa, Katherine
Gelb, Jeff
Walker, Sharon L.
Nisbet, Roger M.
An, Youn-Joo
Schimel, Joshua P.
Palmer, Reid G.
Hernandez-Viezcas, Jose A.
Zhao, Lijuan
Gardea-Torresdey, Jorge L.
Holden, Patricia A.
TI Soybean susceptibility to manufactured nanomaterials with evidence for
food quality and soil fertility interruption
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE nanoparticles; nanotechnology; agriculture
ID WASTE-WATER; CEO2 NANOPARTICLES; NITROGEN-CYCLE; PLANTS; BIOSOLIDS;
TITANIUM; SLUDGE; PHYTOTOXICITY; ACCUMULATION; FIXATION
AB Based on previously published hydroponic plant, planktonic bacterial, and soil microbial community research, manufactured nanomaterial (MNM) environmental buildup could profoundly alter soil-based food crop quality and yield. However, thus far, no single study has at once examined the full implications, as no studies have involved growing plants to full maturity in MNM-contaminated field soil. We have done so for soybean, a major global commodity crop, using farm soil amended with two high-production metal oxide MNMs (nano-CeO2 and -ZnO). The results provide a clear, but unfortunate, view of what could arise over the long term: (i) for nano-ZnO, component metal was taken up and distributed throughout edible plant tissues; (ii) for nano-CeO2, plant growth and yield diminished, but also (iii) nitrogen fixation-a major ecosystem service of leguminous crops-was shut down at high nano-CeO2 concentration. Juxtaposed against widespread land application of wastewater treatment biosolids to food crops, these findings forewarn of agriculturally associated human and environmental risks from the accelerating use of MNMs.
C1 [Priester, John H.; Ge, Yuan; Mielke, Randall E.; Horst, Allison M.; Holden, Patricia A.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
[Priester, John H.; Ge, Yuan; Mielke, Randall E.; Horst, Allison M.; Moritz, Shelly Cole; Nisbet, Roger M.; Schimel, Joshua P.; Holden, Patricia A.] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Priester, John H.; Ge, Yuan; Mielke, Randall E.; Horst, Allison M.; Nisbet, Roger M.; Schimel, Joshua P.; Hernandez-Viezcas, Jose A.; Zhao, Lijuan; Gardea-Torresdey, Jorge L.; Holden, Patricia A.] Univ Calif Santa Barbara, Ctr Environm Implicat Nanotechnol, Santa Barbara, CA 93106 USA.
[Mielke, Randall E.] CALTECH, Div Geol & Planetary Sci, NASA Jet Prop Lab, Pasadena, CA 91101 USA.
[Espinosa, Katherine; Palmer, Reid G.] Iowa State Univ, Dept Agron, Ames, IA 50011 USA.
[Gelb, Jeff] Xradia, Pleasanton, CA 94588 USA.
[Walker, Sharon L.] Univ Calif Riverside, Dept Chem & Environm Engn, Riverside, CA 92521 USA.
[Nisbet, Roger M.; Schimel, Joshua P.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[An, Youn-Joo] Konkuk Univ, Dept Environm Sci, Seoul 143701, South Korea.
[Palmer, Reid G.] ARS, Corn Insects & Crop Genet Res Unit, USDA, Ames, IA 50011 USA.
[Hernandez-Viezcas, Jose A.; Zhao, Lijuan; Gardea-Torresdey, Jorge L.] Univ Texas El Paso, Dept Chem, El Paso, TX 79968 USA.
RP Holden, PA (reprint author), Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
EM holden@bren.ucsb.edu
RI Zhao, Lijuan/E-8485-2012; Nisbet, Roger/B-6951-2014; Ge,
Yuan/D-2997-2009
OI Ge, Yuan/0000-0003-0234-5638
FU National Science Foundation (NSF); Environmental Protection Agency
[DBI-0830117]; NSF [BES-9977772, DBI-0216480]
FX The authors thank Olivier Brun, Carla D'Antonio, Max Moritz, Laurie Van
De Werfhorst, Tom Shepherd, Corrine Dorais, Sadie Iverson, James Cooper,
Gary Stacey, Joan Calder, Alia Servin, and Fabiola Moreno for their
assistance; Michael Guthrie for assistance in experimental design and
implementation; and the three anonymous reviewers of this manuscript.
This research was primarily funded by the National Science Foundation
(NSF) and the Environmental Protection Agency under Cooperative
Agreement DBI-0830117 (to P.A.H, S.L.W., J.P.S, R.M.N., and J.L.G-T.).
Environmental scanning and scanning transmission EM were partly
performed in the Micro-Environmental Imaging and Analysis Facility at
the University of California at Santa Barbara
(https://www.bren.ucsb.edu/facilities/MEIAF/) under NSF Awards
BES-9977772 and DBI-0216480.
NR 44
TC 98
Z9 104
U1 14
U2 187
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD SEP 11
PY 2012
VL 109
IS 37
BP E2451
EP E2456
DI 10.1073/pnas.1205431109
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 012AP
UT WOS:000309208000009
PM 22908279
ER
PT J
AU Painter, TH
Bryant, AC
Skiles, SM
AF Painter, Thomas H.
Bryant, Ann C.
Skiles, S. McKenzie
TI Radiative forcing by light absorbing impurities in snow from MODIS
surface reflectance data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EOLIAN DUST DEPOSITION; SPECTRAL ALBEDO; GRAIN-SIZE; CLIMATE; COVER;
MODEL; ASIA
AB The episodic deposition of dust and carbonaceous particles to snow decreases snow surface albedo and enhances absorption of solar radiation, leading to accelerated snow-melt, negative glacier mass balance, and the snow-albedo feedback. Until now, no remote sensing retrieval has captured the spatial and temporal variability of this forcing. Here we present the MODIS Dust Radiative Forcing in Snow (MODDRFS) model that retrieves surface radiative forcing by light absorbing impurities in snow cover from Moderate Resolution Imaging Spectroradiometer (MODIS) surface reflectance data. Validation of MODDRFS with a 7-year record of in situ measurements indicates the radiative forcing retrieval has positive bias at lower values and slight negative bias above 200 W m(-2), subject to mixed pixel uncertainties. With bias-correction, MODDRFS has a root mean squared error of 32 W m(-2) and mean absolute error of 25 W m(-2). We demonstrate MODDRFS in the Upper Colorado River Basin and Hindu Kush-Himalaya. Citation: Painter, T. H., A. C. Bryant, and S. M. Skiles (2012), Radiative forcing by light absorbing impurities in snow from MODIS surface reflectance data, Geophys. Res. Lett., 39, L17502, doi:10.1029/2012GL052457.
C1 [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bryant, Ann C.] Univ Utah, Dept Geog, Salt Lake City, UT USA.
[Skiles, S. McKenzie] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
RP Painter, TH (reprint author), CALTECH, Jet Prop Lab, M-S 233-306D,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM thomas.painter@jpl.nasa.gov
RI Painter, Thomas/B-7806-2016
FU NSF [ATM04323237]; NASA [NNX10A097G, NNX09A038HS01]; Jet Propulsion
Laboratory, California Institute of Technology
FX This work was funded by NSF grant ATM04323237 and NASA projects
NNX10A097G and NNX09A038HS01. Part of this work was performed at the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA.
NR 27
TC 29
Z9 29
U1 2
U2 36
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 11
PY 2012
VL 39
AR L17502
DI 10.1029/2012GL052457
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 007LP
UT WOS:000308890100001
ER
PT J
AU Liu, D
Gubarev, MV
Resta, G
Ramsey, BD
Moncton, DE
Khaykovich, B
AF Liu, D.
Gubarev, M. V.
Resta, G.
Ramsey, B. D.
Moncton, D. E.
Khaykovich, B.
TI Axisymmetric grazing-incidence focusing optics for small-angle neutron
scattering
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Atom and neutron optics; X-ray optics; Small-angle neutron scattering
ID RESOLUTION; INSTRUMENTS; DIFFRACTOMETER; TECHNOLOGY; LENS
AB We propose and design novel axisymmetric focusing mirrors, known as Wolter optics, for small-angle neutron scattering instruments. Ray-tracing simulations show that using the mirrors can result in more than an order-of-magnitude increase in the neutron flux reaching detectors, while decreasing the minimum wave vector transfer. Such mirrors are made of Ni using a mature technology. They can be coated with neutron supermirror multilayers, and multiple mirrors can be nested to improve their flux-collection ability. Thus, these mirrors offer simple and flexible means of significantly improving existing and future SANS instruments. In addition. short SANS instruments might become possible, especially at compact neutron sources, when high-resolution detectors are combined with Wolter optics. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Liu, D.; Moncton, D. E.; Khaykovich, B.] MIT, Nucl Reactor Lab, Cambridge, MA 02139 USA.
[Gubarev, M. V.; Ramsey, B. D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Resta, G.; Moncton, D. E.] MIT, Dept Phys, Cambridge, MA 02139 USA.
RP Khaykovich, B (reprint author), MIT, Nucl Reactor Lab, 138 Albany St, Cambridge, MA 02139 USA.
EM bkh@mit.edu
RI Khaykovich, Boris/A-7376-2012; Liu, Dazhi/G-2675-2013
OI Khaykovich, Boris/0000-0002-9490-2771; Liu, Dazhi/0000-0002-7604-6940
FU US Department of Energy, Office of Basic Energy Sciences, Division of
Materials Sciences and Engineering [DE-FG02-09ER46556,
DE-FG02-09ER46557]; National Science Foundation [DMR-0526754]
FX We are grateful to Professor Jeffrey Gordon of Ben-Gurion University
(Israel) and Dr. David Mildner of NIST for discussions. Research
supported by the US Department of Energy, Office of Basic Energy
Sciences, Division of Materials Sciences and Engineering under Award
nos. DE-FG02-09ER46556 and DE-FG02-09ER46557 (Wolter optics studies) and
by National Science Foundation under Award no. DMR-0526754 (construction
of Neutron optics test station and diffractometer at MIT).
NR 28
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U1 0
U2 18
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD SEP 11
PY 2012
VL 686
BP 145
EP 150
DI 10.1016/j.nima.2012.05.056
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 983BL
UT WOS:000307091100021
ER
PT J
AU Bussmann, RS
Gurwell, MA
Fu, H
Smith, DJB
Dye, S
Auld, R
Baes, M
Baker, AJ
Bonfield, D
Cava, A
Clements, DL
Cooray, A
Coppin, K
Dannerbauer, H
Dariush, A
De Zotti, G
Dunne, L
Eales, S
Fritz, J
Hopwood, R
Ibar, E
Ivison, RJ
Jarvis, MJ
Kim, S
Leeuw, LL
Maddox, S
Michallowski, MJ
Negrello, M
Pascale, E
Pohlen, M
Riechers, DA
Rigby, E
Scott, D
Temi, P
Van der Werf, PP
Wardlow, J
Wilner, D
Verma, A
AF Bussmann, R. S.
Gurwell, M. A.
Fu, Hai
Smith, D. J. B.
Dye, S.
Auld, R.
Baes, M.
Baker, A. J.
Bonfield, D.
Cava, A.
Clements, D. L.
Cooray, A.
Coppin, K.
Dannerbauer, H.
Dariush, A.
De Zotti, G.
Dunne, L.
Eales, S.
Fritz, J.
Hopwood, R.
Ibar, E.
Ivison, R. J.
Jarvis, M. J.
Kim, S.
Leeuw, L. L.
Maddox, S.
Michallowski, M. J.
Negrello, M.
Pascale, E.
Pohlen, M.
Riechers, D. A.
Rigby, E.
Scott, Douglas
Temi, P.
Van der Werf, P. P.
Wardlow, J.
Wilner, D.
Verma, A.
TI A DETAILED GRAVITATIONAL LENS MODEL BASED ON SUBMILLIMETER ARRAY AND
KECK ADAPTIVE OPTICS IMAGING OF A HERSCHEL-ATLAS SUBMILLIMETER GALAXY AT
z=4.243
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: fundamental parameters; galaxies:
high-redshift; gravitational lensing: strong
ID STAR-FORMATION HISTORY; SCIENCE DEMONSTRATION PHASE; ULTRALUMINOUS
INFRARED GALAXIES; SPACE-TELESCOPE MORPHOLOGIES; DEGREE EXTRAGALACTIC
SURVEY; DEEP-FIELD-SOUTH; ALL-SKY SURVEY; MOLECULAR GAS; BILLION YEARS;
LUMINOSITY FUNCTIONS
AB We present high-spatial resolution imaging obtained with the Submillimeter Array (SMA) at 880 mu m and the Keck adaptive optics (AO) system at the K-S-band of a gravitationally lensed submillimeter galaxy (SMG) at z = 4.243 discovered in the Herschel Astrophysical Terahertz Large Area Survey. The SMA data (angular resolution approximate to 0.'' 6) resolve the dust emission into multiple lensed images, while the Keck AO KS-band data (angular resolution approximate to 0.'' 1) resolve the lens into a pair of galaxies separated by 0.'' 3. We present an optical spectrum of the foreground lens obtained with the Gemini-South telescope that provides a lens redshift of z(lens) = 0.595 +/- 0.005. We develop and apply a new lens modeling technique in the visibility plane that shows that the SMG is magnified by a factor of mu = 4.1 +/- 0.2 and has an intrinsic infrared (IR) luminosity of L-IR = (2.1 +/- 0.2) x 10(13) L-circle dot. We measure a half-light radius of the background source of r(s) = 4.4 +/- 0.5 kpc which implies an IR luminosity surface density of Sigma(IR) = (3.4 +/- 0.9) x 10(11) L-circle dot kpc(-2), a value that is typical of z > 2 SMGs but significantly lower than IR luminous galaxies at z similar to 0. The two lens galaxies are compact (r(lens) approximate to 0.9 kpc) early-types with Einstein radii of theta(E1) = 0.57 +/- 0.01 and theta(E2) = 0.40 +/- 0.01 that imply masses of M-lens1 = (7.4 +/- 0.5) x 10(10) M-circle dot and M-lens2 = (3.7 +/- 0.3) x 10(10) M-circle dot. The two lensing galaxies are likely about to undergo a dissipationless merger, and the mass and size of the resultant system should be similar to other early-type galaxies at z similar to 0.6. This work highlights the importance of high spatial resolution imaging in developing models of strongly lensed galaxies discovered by Herschel.
C1 [Bussmann, R. S.; Gurwell, M. A.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fu, Hai; Cooray, A.; Kim, S.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Smith, D. J. B.; Bonfield, D.; Dunne, L.; Jarvis, M. J.; Maddox, S.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England.
[Dye, S.; Eales, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Auld, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Clements, D. L.; Dariush, A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Coppin, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Dannerbauer, H.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[De Zotti, G.; Negrello, M.] Univ Padua, Dipto Astron, IT-35122 Padua, Italy.
[Hopwood, R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
[Leeuw, L. L.] Univ Johannesburg, Dept Phys, Auckland Pk 2006, South Africa.
[Michallowski, M. J.] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Pascale, E.; Pohlen, M.] ESO, D-85748 Garching, Germany.
[Riechers, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Rigby, E.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Temi, P.] NASA, Space Sci & Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Verma, A.] Univ Oxford, Oxford OX1 3RH, England.
RP Bussmann, RS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rbussmann@cfa.harvard.edu
RI Baes, Maarten/I-6985-2013; Wardlow, Julie/C-9903-2015; Ivison,
R./G-4450-2011; Cava, Antonio/C-5274-2017;
OI Dye, Simon/0000-0002-1318-8343; Baes, Maarten/0000-0002-3930-2757;
Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313;
Cava, Antonio/0000-0002-4821-1275; De Zotti,
Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X;
Scott, Douglas/0000-0002-6878-9840; Smith, Daniel/0000-0001-9708-253X;
/0000-0002-0729-2988
FU Smithsonian Institution; Academia Sinica; W. M. Keck Foundation; NASA
from JPL; SMA Fellowship program; NSF CAREER [AST-0645427]
FX Some of the data presented herein were obtained at the Submillimeter
Array, which 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.; 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 results described in this paper are based on
observations obtained with Herschel, an ESA space observatory with
science instruments provided by European-led Principal Investigator
consortia and with important participation from NASA. The Herschel-ATLAS
is a project with Herschel, which is an ESA space observatory with
science instruments provided by European-led Principal Investigator
consortia and with important participation from NASA. The H-ATLAS Web
site is http://www.h-atlas.org/. US participants in H-ATLAS acknowledge
support from NASA through a contract from JPL. R. S. B. acknowledges
support from the SMA Fellowship program. H. F., A. C., J.L.W., and S. K.
acknowledge support from NSF CAREER AST-0645427. We thank K. Rosenfeld
and S. M. Andrews for assistance in implementing the lens modeling
analysis in the visibility plane. We thank the referee for a thorough
review of the manuscript which resulted in a stronger paper overall.
NR 88
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U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 134
DI 10.1088/0004-637X/756/2/134
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200030
ER
PT J
AU Chiang, HF
Looney, LW
Tobin, JJ
AF Chiang, Hsin-Fang
Looney, Leslie W.
Tobin, John J.
TI THE ENVELOPE AND EMBEDDED DISK AROUND THE CLASS 0 PROTOSTAR L1157-mm:
DUAL-WAVELENGTH INTERFEROMETRIC OBSERVATIONS AND MODELING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation; stars: protostars; techniques: interferometric
ID T-TAURI STARS; YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS;
PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; MILLIMETER WAVELENGTHS; SIZE
DISTRIBUTION; GRAIN-GROWTH; SUBMILLIMETER ARRAY; SUBARCSECOND SURVEY
AB We present dual-wavelength observations and modeling of the nearly edge-on Class 0 young stellar object L1157-mm. Using the Combined Array for Research in Millimeter-wave Astronomy, a nearly spherical structure is seen from the circumstellar envelope at the size scale of 10(2)-10(3) AU in both 1 mm and 3 mm dust emission. Radiative transfer modeling is performed to compare data with theoretical envelope models, including a power-law envelope model and the Terebey-Shu-Cassen model. Bayesian inference is applied for parameter estimation and information criterion is used for model selection. The results prefer the power-law envelope model against the Terebey-Shu-Cassen model. In particular, for the power-law envelope model, a steep density profile with an index of similar to 2 is inferred. Moreover, the dust opacity spectral index beta is estimated to be similar to 0.9, implying that grain growth has started at L1157-mm. Also, the unresolved disk component is constrained to be less than or similar to 40 AU in radius and less than or similar to 4-25 M-Jup in mass. However, the estimate of the embedded disk component relies on the assumed envelope model.
C1 [Chiang, Hsin-Fang; Looney, Leslie W.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Chiang, Hsin-Fang] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA.
[Chiang, Hsin-Fang] NASA, Astrobiol Inst, Ames Res Ctr, Mountain View, CA USA.
[Tobin, John J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
RP Chiang, HF (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
EM hchiang@ifa.hawaii.edu
FU Laboratory for Astronomical Imaging at the University of Illinois; NSF
[AST-07-09206]; NASA through Hubble Fellowship [HF-51300.01]; Space
Telescope Science Institute; NASA [NAS 5-26555]
FX The authors thank B. Reipurth and the anonymous referee for their
careful reading of the manuscript and helpful comments. H.-F.C. and L.
W. L. acknowledge support from the Laboratory for Astronomical Imaging
at the University of Illinois and the NSF under grant AST-07-09206. J.T.
acknowledges support provided by NASA through Hubble Fellowship grant
HF-51300.01 awarded by the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., for NASA, under contract NAS 5-26555. We also thank CARMA staff
and observers for their assistance in obtaining the data. Support for
CARMA construction was derived from the states of Illinois, California,
and Maryland, the James S. McDonnell Foundation, the Gordon and Betty
Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the
University of Chicago, the Associates of the California Institute of
Technology, and the National Science Foundation. Ongoing CARMA
development and operations are supported by the National Science
Foundation under a cooperative agreement, and by the CARMA partner
universities.
NR 107
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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 SEP 10
PY 2012
VL 756
IS 2
AR 168
DI 10.1088/0004-637X/756/2/168
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200064
ER
PT J
AU Evans, RM
Opher, M
Oran, R
van der Holst, B
Sokolov, IV
Frazin, R
Gombosi, TI
Vasquez, A
AF Evans, R. M.
Opher, M.
Oran, R.
van der Holst, B.
Sokolov, I. V.
Frazin, R.
Gombosi, T. I.
Vasquez, A.
TI CORONAL HEATING BY SURFACE ALFVEN WAVE DAMPING: IMPLEMENTATION IN A
GLOBAL MAGNETOHYDRODYNAMICS MODEL OF THE SOLAR WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; magnetohydrodynamics (MHD); solar wind; Sun: corona;
waves
ID OPEN MAGNETIC CONFIGURATIONS; EMISSION MEASURE TOMOGRAPHY; PROPAGATING
KINK WAVES; II RADIO-BURSTS; RESONANT ABSORPTION; LOOP OSCILLATIONS;
INTERPLANETARY MEDIUM; PLASMA PARAMETERS; TRANSITION REGION; CYCLOTRON
WAVES
AB The heating and acceleration of the solar wind is an active area of research. Alfven waves, because of their ability to accelerate and heat the plasma, are a likely candidate in both processes. Many models have explored wave dissipation mechanisms which act either in closed or open magnetic field regions. In this work, we emphasize the boundary between these regions, drawing on observations which indicate unique heating is present there. We utilize a new solar corona component of the Space Weather Modeling Framework, in which Alfven wave energy transport is self-consistently coupled to the magnetohydrodynamic equations. In this solar wind model, the wave pressure gradient accelerates and wave dissipation heats the plasma. Kolmogorov-like wave dissipation as expressed by Hollweg along open magnetic field lines was presented in van der Holst et al. Here, we introduce an additional dissipation mechanism: surface Alfven wave (SAW) damping, which occurs in regions with transverse (with respect to the magnetic field) gradients in the local Alfven speed. For solar minimum conditions, we find that SAW dissipation is weak in the polar regions (where Hollweg dissipation is strong), and strong in subpolar latitudes and the boundaries of open and closed magnetic fields (where Hollweg dissipation is weak). We show that SAW damping reproduces regions of enhanced temperature at the boundaries of open and closed magnetic fields seen in tomographic reconstructions in the low corona. Also, we argue that Ulysses data in the heliosphere show enhanced temperatures at the boundaries of fast and slow solar wind, which is reproduced by SAW dissipation. Therefore, the model's temperature distribution shows best agreement with these observations when both dissipation mechanisms are considered. Lastly, we use observational constraints of shock formation in the low corona to assess the Alfven speed profile in the model. We find that, compared to a polytropic solar wind model, the wave-driven model with physical dissipation mechanisms presented in this work is more aligned with an empirical Alfven speed profile. Therefore, a wave-driven model which includes the effects of SAW damping is a better background to simulate coronal-mass-ejection-driven shocks.
C1 [Evans, R. M.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Evans, R. M.; Opher, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Oran, R.; van der Holst, B.; Sokolov, I. V.; Frazin, R.; Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
[Vasquez, A.] Inst Astron & Fis Espacio CONICET UBA, Buenos Aires, DF, Argentina.
[Vasquez, A.] FCEN UBA, Buenos Aires, DF, Argentina.
RP Evans, RM (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
EM Rebekah.e.frolov@nasa.gov
RI Frazin, Richard/J-2625-2012; Gombosi, Tamas/G-4238-2011; Sokolov,
Igor/H-9860-2013; van der Holst, Bart/A-3557-2013;
OI Gombosi, Tamas/0000-0001-9360-4951; Sokolov, Igor/0000-0002-6118-0469;
van der Holst, Bart/0000-0001-5260-3944; Oran, Rona/0000-0001-6419-552X
FU NSF [ATM 0747654]
FX We thank NASA Ames for use of the Pleiades supercomputer. R. E. thanks
an anonymous referee for the comments and suggestions that greatly
improved the manuscript. This research was supported in part by NSF
CAREER Grant ATM 0747654, and in part by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by Oak
Ridge Associated Universities through a contract with NASA.
NR 107
TC 16
Z9 16
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 SEP 10
PY 2012
VL 756
IS 2
AR 155
DI 10.1088/0004-637X/756/2/155
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200051
ER
PT J
AU Fong, W
Berger, E
Margutti, R
Zauderer, BA
Troja, E
Czekala, I
Chornock, R
Gehrels, N
Sakamoto, T
Fox, DB
Podsiadlowski, P
AF Fong, W.
Berger, E.
Margutti, R.
Zauderer, B. A.
Troja, E.
Czekala, I.
Chornock, R.
Gehrels, N.
Sakamoto, T.
Fox, D. B.
Podsiadlowski, P.
TI A JET BREAK IN THE X-RAY LIGHT CURVE OF SHORT GRB 111020A: IMPLICATIONS
FOR ENERGETICS AND RATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst: individual (111020A)
ID NEUTRON-STAR BINARIES; COMPACT OBJECT MERGERS; LATE-TIME AFTERGLOW;
SWIFT XRT DATA; GAMMA-RAY; BURST AFTERGLOWS; BLACK-HOLES; HOST GALAXIES;
OBSERVATIONAL CONSTRAINTS; TELESCOPE OBSERVATIONS
AB We present broadband observations of the afterglow and environment of the short GRB 111020A. An extensive X-ray light curve from Swift/XRT, XMM-Newton, and Chandra, spanning similar to 100 s to 10 days after the burst, reveals a significant break at delta t approximate to 2 days with pre- and post-break decline rates of alpha(X, 1) approximate to -0.78 and alpha(X, 2) less than or similar to -1.7, respectively. Interpreted as a jet break, we infer a collimated outflow with an opening angle of theta(j) approximate to 3 degrees-8 degrees. The resulting beaming-corrected gamma-ray (10-1000 keV band) and blast-wave kinetic energies are (2-3) x 10(48) erg and (0.3-2) x 10(49) erg, respectively, with the range depending on the unknown redshift of the burst. We report a radio afterglow limit of <39 mu Jy (3 sigma) from Expanded Very Large Array observations that, along with our finding that nu(c) < nu(X), constrains the circumburst density to n(0) similar to 0.01-0.1 cm(-3). Optical observations provide an afterglow limit of i greater than or similar to 24.4 mag at 18 hr after the burst and reveal a potential host galaxy with i approximate to 24.3 mag. The subarcsecond localization from Chandra provides a precise offset of 0 ''.80+/-0 ''.11 (1 sigma) from this galaxy corresponding to an offset of 5-7 kpc for z = 0.5-1.5. We find a high excess neutral hydrogen column density of (7.5 +/- 2.0) x 10(21) cm(-2) (z = 0). Our observations demonstrate that a growing fraction of short gamma-ray bursts (GRBs) are collimated, which may lead to a true event rate of greater than or similar to 100-1000 Gpc(-3) yr(-1), in good agreement with the NS-NS merger rate of approximate to 200-3000 Gpc(-3) yr(-1). This consistency is promising for coincident short GRB-gravitational wave searches in the forthcoming era of Advanced LIGO/VIRGO.
C1 [Fong, W.; Berger, E.; Margutti, R.; Zauderer, B. A.; Czekala, I.; Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Troja, E.; Gehrels, N.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Podsiadlowski, P.] Univ Oxford, Dept Astron, Oxford OX1 3RH, England.
RP Fong, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Czekala, Ian/0000-0002-1483-8811
FU National Science Foundation [AST-1107973]; National Aeronautics and
Space Administration through Chandra X-Ray Observatory Center
[GO1-12072X]; National Aeronautics Space Administration [NAS8-03060];
NASA/Swift AO6 grant [NNX10AI24G]
FX We thank D. Finkbeiner for helpful discussions. The Berger GRB group at
Harvard is supported by the National Science Foundation under grant
AST-1107973. Partial support was also provided by the National
Aeronautics and Space Administration through Chandra Award Number
GO1-12072X issued by the Chandra X-Ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of the National Aeronautics Space Administration under contract
NAS8-03060. Additional support was provided by NASA/Swift AO6 grant
NNX10AI24G. Observations were obtained with the EVLA (Program 10C-145)
operated by the National Radio Astronomy Observatory, a facility of the
National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. This paper includes data gathered with the
6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
This work is based in part on observations obtained at the Gemini
Observatory, which is operated by the Association of Universities for
Research in Astronomy, Inc., under a cooperative agreement with the NSF
on behalf of the Gemini partnership: the National Science Foundation
(United States), the 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).
NR 109
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 189
DI 10.1088/0004-637X/756/2/189
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200085
ER
PT J
AU Ford, EB
Ragozzine, D
Rowe, JF
Steffen, JH
Barclay, T
Batalha, NM
Borucki, WJ
Bryson, ST
Caldwell, DA
Fabrycky, DC
Gautier, TN
Holman, MJ
Ibrahim, KA
Kjeldsen, H
Kinemuchi, K
Koch, DG
Lissauer, JJ
Still, M
Tenenbaum, P
Uddin, K
Welsh, W
AF Ford, Eric B.
Ragozzine, Darin
Rowe, Jason F.
Steffen, Jason H.
Barclay, Thomas
Batalha, Natalie M.
Borucki, William J.
Bryson, Stephen T.
Caldwell, Douglas A.
Fabrycky, Daniel C.
Gautier, Thomas N., III
Holman, Matthew J.
Ibrahim, Khadeejah A.
Kjeldsen, Hans
Kinemuchi, Karen
Koch, David G.
Lissauer, Jack J.
Still, Martin
Tenenbaum, Peter
Uddin, Kamal
Welsh, William
TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. V. TRANSIT TIMING VARIATION
CANDIDATES IN THE FIRST SIXTEEN MONTHS FROM POLYNOMIAL MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: detection; planets and
satellites: dynamical evolution and stability; techniques: miscellaneous
ID MULTIPLE-PLANET SYSTEMS; SUN-LIKE STAR; HIERARCHICAL TRIPLE; LOW-MASS;
CONFIRMATION; ARCHITECTURE; PHOTOMETRY
AB Transit timing variations provide a powerful tool for confirming and characterizing transiting planets, as well as detecting non-transiting planets. We report the results of an updated transit timing variation (TTV) analysis for 1481 planet candidates based on transit times measured during the first sixteen months of Kepler observations. We present 39 strong TTV candidates based on long-term trends (2.8% of suitable data sets). We present another 136 weaker TTV candidates (9.8% of suitable data sets) based on the excess scatter of TTV measurements about a linear ephemeris. We anticipate that several of these planet candidates could be confirmed and perhaps characterized with more detailed TTV analyses using publicly available Kepler observations. For many others, Kepler has observed a long-term TTV trend, but an extended Kepler mission will be required to characterize the system via TTVs. We find that the occurrence rate of planet candidates that show TTVs is significantly increased (similar to 68%) for planet candidates transiting stars with multiple transiting planet candidates when compared to planet candidates transiting stars with a single transiting planet candidate.
C1 [Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
[Ragozzine, Darin; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ibrahim, Khadeejah A.; Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rowe, Jason F.; Caldwell, Douglas A.; Tenenbaum, Peter] SETI Inst, Mountain View, CA 94043 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Barclay, Thomas; Kinemuchi, Karen; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Welsh, William] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Ford, EB (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
EM eford@astro.ufl.edu
RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014;
OI Barclay, Thomas/0000-0001-7139-2724; Fabrycky,
Daniel/0000-0003-3750-0183; Caldwell, Douglas/0000-0003-1963-9616;
/0000-0001-6545-639X
FU NASA's Science Mission Directorate; National Aeronautics and Space
Administration [NNX08AR04G]
FX Funding for this mission is provided by NASA's Science Mission
Directorate. We thank the entire Kepler team for the many years of work
that is proving so successful. E.B.F. acknowledges support by the
National Aeronautics and Space Administration under grant NNX08AR04G
issued through the Kepler Participating Scientist Program.
NR 25
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 185
DI 10.1088/0004-637X/756/2/185
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200081
ER
PT J
AU Morley, CV
Fortney, JJ
Marley, MS
Visscher, C
Saumon, D
Leggett, SK
AF Morley, Caroline V.
Fortney, Jonathan J.
Marley, Mark S.
Visscher, Channon
Saumon, Didier
Leggett, S. K.
TI NEGLECTED CLOUDS IN T AND Y DWARF ATMOSPHERES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: atmospheres
ID EXTRASOLAR GIANT PLANETS; COLLISION-INDUCED ABSORPTION; COOL BROWN
DWARF; HR 8799 PLANETS; GLIESE 229B; MODEL ATMOSPHERES; MU-M;
CHEMICAL-EQUILIBRIUM; DUSTY PHOTOSPHERES; SYNTHETIC SPECTRA
AB As brown dwarfs cool, a variety of species condense in their atmospheres, forming clouds. Iron and silicate clouds shape the emergent spectra of L dwarfs, but these clouds dissipate at the L/T transition. A variety of other condensates are expected to form in cooler T dwarf atmospheres. These include Cr, MnS, Na2S, ZnS, and KCl, but the opacity of these optically thinner clouds has not been included in previous atmosphere models. Here, we examine their effect on model T and Y dwarf atmospheres. The cloud structures and opacities are calculated using the Ackerman & Marley cloud model, which is coupled to an atmosphere model to produce atmospheric pressure-temperature profiles in radiative-convective equilibrium. We generate a suite of models between T-eff = 400 and 1300 K, log g = 4.0 and 5.5, and condensate sedimentation efficiencies from f(sed) = 2 to 5. Model spectra are compared to two red T dwarfs, Ross 458C and UGPS 0722-05; models that include clouds are found to match observed spectra significantly better than cloudless models. The emergence of sulfide clouds in cool atmospheres, particularly (NaS)-S-2, may be a more natural explanation for the "cloudy" spectra of these objects, rather than the reemergence of silicate clouds that wane at the L-to-T transition. We find that sulfide clouds provide a mechanism to match the near-and mid-infrared colors of observed T dwarfs. Our results indicate that including the opacity of condensates in T dwarf atmospheres is necessary to accurately determine the physical characteristics of many of the observed objects.
C1 [Morley, Caroline V.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Visscher, Channon] SW Res Inst, Boulder, CO 80302 USA.
[Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Leggett, S. K.] No Operat Ctr, Gemini Observ, Hilo, HI 96720 USA.
RP Morley, CV (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM cmorley@ucolick.org
RI Marley, Mark/I-4704-2013;
OI Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943;
Leggett, Sandy/0000-0002-3681-2989
NR 92
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 172
DI 10.1088/0004-637X/756/2/172
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200068
ER
PT J
AU Musella, I
Ripepi, V
Marconi, M
Clementini, G
Dall'Ora, M
Scowcroft, V
Moretti, MI
Di Fabrizio, L
Greco, C
Coppola, G
Bersier, D
Catelan, M
Grado, A
Limatola, L
Smith, HA
Kinemuchi, K
AF Musella, Ilaria
Ripepi, Vincenzo
Marconi, Marcella
Clementini, Gisella
Dall'Ora, Massimo
Scowcroft, Victoria
Moretti, Maria Ida
Di Fabrizio, Luca
Greco, Claudia
Coppola, Giuseppina
Bersier, David
Catelan, Marcio
Grado, Aniello
Limatola, Luca
Smith, Horace A.
Kinemuchi, Karen
TI STELLAR ARCHEOLOGY IN THE GALACTIC HALO WITH ULTRA-FAINT DWARFS. VII.
HERCULES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: individual (Hercules); stars: distances;
stars: variables: general; stars: variables: RR Lyrae; techniques:
photometric
ID RR-LYRAE VARIABLES; PHOTOMETRIC STANDARD STARS; MILKY-WAY SATELLITE;
MULTIELEMENT ABUNDANCE MEASUREMENTS; HORIZONTAL-BRANCH STARS;
GLOBULAR-CLUSTER M3; BVI CCD PHOTOMETRY; SPHEROIDAL GALAXY; POPULATION
SYNTHESIS; EVOLUTION DATABASE
AB We present the first time-series study of the ultra-faint dwarf galaxy Hercules. Using a variety of telescope/instrument facilities we secured about 50 V and 80 B epochs. These data allowed us to detect and characterize 10 pulsating variable stars in Hercules. Our final sample includes six fundamental-mode (ab-type) and three first-overtone (c-type) RR Lyrae stars, and one Anomalous Cepheid. The average period of the ab-type RR Lyrae stars, < P-ab > = 0.68 days (sigma = 0.03 days), places Hercules in the Oosterhoff II group, as found for almost the totality of the ultra-faint dwarf galaxies investigated so far for variability. The RR Lyrae stars were used to obtain independent estimates of the metallicity, reddening, and distance to Hercules, for which we find [Fe/H] = -2.30 +/- 0.15 dex, E(B - V) = 0.09 +/- 0.02 mag, and (m - M)(0) = 20.6 +/- 0.1 mag, in good agreement with the literature values. We have obtained a V, B - V color-magnitude diagram (CMD) of Hercules that reaches V similar to 25 mag and extends beyond the galaxy's half-light radius over a total area of 40' x 36'. The CMD and the RR Lyrae stars indicate the presence of a population as old and metal-poor as (at least) the Galactic globular cluster M68.
C1 [Musella, Ilaria; Ripepi, Vincenzo; Marconi, Marcella; Dall'Ora, Massimo; Coppola, Giuseppina; Grado, Aniello; Limatola, Luca] Osserv Astron Capodimonte, INAF, I-8013 Naples, Italy.
[Clementini, Gisella] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Scowcroft, Victoria] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Scowcroft, Victoria; Bersier, David] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH4 1LD, Merseyside, England.
[Moretti, Maria Ida] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Di Fabrizio, Luca] Ctr Galileo Galilei & Telescopio Nazl Galileo, INAF, E-38700 S Cruz De La Palma, Spain.
[Greco, Claudia] Observ Geneva, CH-1290 Sauverny, Switzerland.
[Catelan, Marcio] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Smith, Horace A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Kinemuchi, Karen] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Musella, I (reprint author), Osserv Astron Capodimonte, INAF, I-8013 Naples, Italy.
EM ilaria@na.astro.it; ripepi@na.astro.it; marcella@na.astro.it;
gisella.clementini@oabo.inaf.it; dallora@na.astro.it;
vs@obs.carnegiescience.edu; mariaida.moretti@studio.unibo.it;
difabrizio@tng.iac.es; claudia.greco@obs.unige.ch; coppola@na.astro.it;
mcatelan@astro.puc.cl; smith@pa.msu.edu; karen.kinemuchi@nasa.gov
RI Moretti, Maria Ida/K-8558-2015;
OI Marconi, Marcella/0000-0002-1330-2927; Musella,
Ilaria/0000-0001-5909-6615; Grado, Aniello/0000-0002-0501-8256
FU COFIS ASI-INAF [I/016/07/0]; ASI-INAF [I/009/10/0]; PRIN INAF (PI: G.
Clementini); Proyecto Fondecyt [1110326]; BASAL Center for Astrophysics
and Associated Technologies [PFB-06]; FONDAP Center for Astrophysics
[15010003]; Chilean Ministry for the Economy, Development, and Tourism's
Programa Iniciativa Cientifica Milenio [P07-021-F]; Milky Way Millennium
Nucleus; Proyecto Anillo; U.S. NSF [AST0607249, AST0707756]
FX We thank an anonymous referee for carefully reading the paper and for
providing comments that helped to improve the clarity of the manuscript.
Financial support for this research was provided by COFIS ASI-INAF
I/016/07/0, by the agreement ASI-INAF I/009/10/0, and by PRIN INAF 2010
(PI: G. Clementini). Support for M. C. is provided by Proyecto Fondecyt
Regular 1110326; BASAL Center for Astrophysics and Associated
Technologies (PFB-06); FONDAP Center for Astrophysics (15010003); the
Chilean Ministry for the Economy, Development, and Tourism's Programa
Iniciativa Cientifica Milenio through grant P07-021-F, awarded to The
Milky Way Millennium Nucleus; and Proyecto Anillo ACT-86. H. A. S.
thanks the U.S. NSF for support under grants AST0607249 and AST0707756.
NR 68
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 121
DI 10.1088/0004-637X/756/2/121
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200017
ER
PT J
AU Postman, M
Lauer, TR
Donahue, M
Graves, G
Coe, D
Moustakas, J
Koekemoer, A
Bradley, L
Ford, HC
Grillo, C
Zitrin, A
Lemze, D
Broadhurst, T
Moustakas, L
Ascaso, B
Medezinski, E
Kelson, D
AF Postman, Marc
Lauer, Tod R.
Donahue, Megan
Graves, Genevieve
Coe, Dan
Moustakas, John
Koekemoer, Anton
Bradley, Larry
Ford, Holland C.
Grillo, Claudio
Zitrin, Adi
Lemze, Doron
Broadhurst, Tom
Moustakas, Leonidas
Ascaso, Begona
Medezinski, Elinor
Kelson, Daniel
TI A BRIGHTEST CLUSTER GALAXY WITH AN EXTREMELY LARGE FLAT CORE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: nuclei; galaxies: photometry; galaxies: structure
ID SUPERMASSIVE BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; STELLAR POPULATION
SYNTHESIS; ACTIVE GALACTIC NUCLEI; ELLIPTIC GALAXIES; FUNDAMENTAL PLANE;
MASS DEFICITS; SKY SURVEY; CENTERS; RESOLUTION
AB Hubble Space Telescope images of the galaxy cluster A2261, obtained as part of the Cluster Lensing And Supernova survey with Hubble, show that the brightest galaxy in the cluster, A2261-BCG, has the largest core yet detected in any galaxy. The cusp radius of A2261-BCG is 3.2 kpc, twice as big as the next largest core known, and similar to 3x bigger than those typically seen in the most luminous brightest cluster galaxies. The morphology of the core in A2261-BCG is also unusual, having a completely flat interior surface brightness profile, rather than the typical shallow cusp rising into the center. This implies that the galaxy has a core with constant or even centrally decreasing stellar density. Interpretation of the core as an end product of the "scouring" action of a binary supermassive black hole implies a total black hole mass similar to 10(10) M-circle dot from the extrapolation of most relationships between core structure and black hole mass. The core falls 1 sigma above the cusp radius versus galaxy luminosity relation. Its large size in real terms, and the extremely large black hole mass required to generate it, raises the possibility that the core has been enlarged by additional processes, such as the ejection of the black holes that originally generated the core. The flat central stellar density profile is consistent with this hypothesis. The core is also displaced by 0.7 kpc from the center of the surrounding envelope, consistent with a local dynamical perturbation of the core.
C1 [Postman, Marc; Coe, Dan; Koekemoer, Anton; Bradley, Larry] Space Telescope Sci Inst, Baltimore, MD 21208 USA.
[Lauer, Tod R.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Graves, Genevieve] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Moustakas, John] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
[Ford, Holland C.; Lemze, Doron; Medezinski, Elinor] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Grillo, Claudio] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Zitrin, Adi] Univ Heidelberg, D-69120 Heidelberg, Germany.
[Broadhurst, Tom] Univ Basque Country UPV EHU, Dept Theoret Phys, E-48940 Leioa, Spain.
[Broadhurst, Tom] Basque Fdn Sci, IKERBASQUE, E-48008 Bilbao, Spain.
[Moustakas, Leonidas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ascaso, Begona] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Kelson, Daniel] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
RP Postman, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21208 USA.
RI Grillo, Claudio/E-6223-2015;
OI Grillo, Claudio/0000-0002-5926-7143; Moustakas,
Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048;
Postman, Marc/0000-0002-9365-7989
FU Association of Universities for Research in Astronomy, Inc. (AURA),
under NASA [NAS 5-26555]; Internationale Spitzenforschung II-1 of the
Baden-Wurttemberg Stiftung
FX We thank David Merritt for useful conversations. 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. (AURA), under NASA contract
NAS 5-26555. The HST observations are associated with GO proposal 12066.
Also based on observations obtained at the Gemini Observatory (acquired
through the Gemini Science Archive), which is operated by the AURA under
a cooperative agreement with the NSF on behalf of the Gemini
partnership: the National Science Foundation (United States); the
Science and Technology Facilities Council (United Kingdom); the National
Research Council (Canada); CONICYT (Chile); the Australian Research
Council (Australia); Ministerio da Ciencia, Tecnologia e Inovacao
(Brazil); and Ministerio de Ciencia, Tecnologia e Innovacion Productiva
(Argentina). A.Z. is supported by contract research Internationale
Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung.
NR 57
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 159
DI 10.1088/0004-637X/756/2/159
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200055
ER
PT J
AU Rawle, TD
Rex, M
Egami, E
Chung, SM
Perez-Gonzalez, PG
Smail, I
Walth, G
Altieri, B
Appleton, P
Alba, AB
Blain, AW
Dessauges-Zavadsky, M
Fadda, D
Gonzalez, AH
Pereira, MJ
Valtchanov, I
van der Werf, PP
Zemcov, M
AF Rawle, T. D.
Rex, M.
Egami, E.
Chung, S. M.
Perez-Gonzalez, P. G.
Smail, I.
Walth, G.
Altieri, B.
Appleton, P.
Alba, A. Berciano
Blain, A. W.
Dessauges-Zavadsky, M.
Fadda, D.
Gonzalez, A. H.
Pereira, M. J.
Valtchanov, I.
van der Werf, P. P.
Zemcov, M.
TI DISCOVERY OF "WARM DUST" GALAXIES IN CLUSTERS AT z similar to 0.3:
EVIDENCE FOR STRIPPING OF COOL DUST IN THE DENSE ENVIRONMENT?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: star formation; infrared:
galaxies
ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; BULLET CLUSTER;
LUMINOSITY FUNCTION; INFRARED GALAXIES; RICH CLUSTERS; DARK-MATTER;
HERSCHEL; EVOLUTION; SUBMILLIMETER
AB Using far-infrared imaging from the "Herschel Lensing Survey," we derive dust properties of spectroscopically confirmed cluster member galaxies within two massive systems at z similar to 0.3: the merging Bullet Cluster and the more relaxed MS2137.3-2353. Most star-forming cluster sources (similar to 90%) have characteristic dust temperatures similar to local field galaxies of comparable infrared (IR) luminosity (T-dust similar to 30 K). Several sub-luminous infrared galaxy (LIRG; L-IR < 10(11) L-circle dot) Bullet Cluster members are much warmer (T-dust > 37 K) with far-infrared spectral energy distribution (SED) shapes resembling LIRG-type local templates. X-ray and mid-infrared data suggest that obscured active galactic nuclei do not contribute significantly to the infrared flux of these "warm dust" galaxies. Sources of comparable IR luminosity and dust temperature are not observed in the relaxed cluster MS2137, although the significance is too low to speculate on an origin involving recent cluster merging. " Warm dust" galaxies are, however, statistically rarer in field samples (> 3 sigma), indicating that the responsible mechanism may relate to the dense environment. The spatial distribution of these sources is similar to the whole far-infrared bright population, i.e., preferentially located in the cluster periphery, although the galaxy hosts tend toward lower stellar masses (M-* < 10(10) M-circle dot). We propose dust stripping and heating processes which could be responsible for the unusually warm characteristic dust temperatures. A normal star-forming galaxy would need 30%-50% of its dust removed (preferentially stripped from the outer reaches, where dust is typically cooler) to recover an SED similar to a "warm dust" galaxy. These progenitors would not require a higher IR luminosity or dust mass than the currently observed normal star-forming population.
C1 [Rawle, T. D.; Rex, M.; Egami, E.; Walth, G.; Pereira, M. J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Chung, S. M.; Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Chung, S. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Perez-Gonzalez, P. G.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Smail, I.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Altieri, B.; Valtchanov, I.] ESA, ESAC, Herschel Sci Ctr, E-28691 Madrid, Spain.
[Appleton, P.; Fadda, D.] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Alba, A. Berciano] ASTRON, NL-7991 PD Dwingeloo, Netherlands.
[Alba, A. Berciano; van der Werf, P. P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Blain, A. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Dessauges-Zavadsky, M.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Zemcov, M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rawle, TD (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
EM trawle@as.arizona.edu
RI Smail, Ian/M-5161-2013; Perez-Gonzalez, Pablo/J-2871-2016;
OI Smail, Ian/0000-0003-3037-257X; Perez-Gonzalez,
Pablo/0000-0003-4528-5639; Altieri, Bruno/0000-0003-3936-0284
FU NASA
FX This work is partially based on observations made with the Herschel
Space Observatory, 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. We also thank the HSC and
NHSC consortia for support with data reduction. This work has made use
of the private version of the Rainbow Cosmological Surveys Database,
which is operated by the Universidad Complutense de Madrid (UCM). We
would also like to thank Maxim Markevitch for providing the Bullet
Cluster X-ray point-source catalog, and Jean-Gabriel Cuby for the
VLT/HAWK-I images.
NR 64
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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 SEP 10
PY 2012
VL 756
IS 2
AR 106
DI 10.1088/0004-637X/756/2/106
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200002
ER
PT J
AU Sanders, NE
Soderberg, AM
Valenti, S
Foley, RJ
Chornock, R
Chomiuk, L
Berger, E
Smartt, S
Hurley, K
Barthelmy, SD
Levesque, EM
Narayan, G
Botticella, MT
Briggs, MS
Connaughton, V
Terada, Y
Gehrels, N
Golenetskii, S
Mazets, E
Cline, T
von Kienlin, A
Boynton, W
Chambers, KC
Grav, T
Heasley, JN
Hodapp, KW
Jedicke, R
Kaiser, N
Kirshner, RP
Kudritzki, RP
Luppino, GA
Lupton, RH
Magnier, EA
Monet, DG
Morgan, JS
Onaka, PM
Price, PA
Stubbs, CW
Tonry, JL
Wainscoat, RJ
Waterson, MF
AF Sanders, N. E.
Soderberg, A. M.
Valenti, S.
Foley, R. J.
Chornock, R.
Chomiuk, L.
Berger, E.
Smartt, S.
Hurley, K.
Barthelmy, S. D.
Levesque, E. M.
Narayan, G.
Botticella, M. T.
Briggs, M. S.
Connaughton, V.
Terada, Y.
Gehrels, N.
Golenetskii, S.
Mazets, E.
Cline, T.
von Kienlin, A.
Boynton, W.
Chambers, K. C.
Grav, T.
Heasley, J. N.
Hodapp, K. W.
Jedicke, R.
Kaiser, N.
Kirshner, R. P.
Kudritzki, R-P.
Luppino, G. A.
Lupton, R. H.
Magnier, E. A.
Monet, D. G.
Morgan, J. S.
Onaka, P. M.
Price, P. A.
Stubbs, C. W.
Tonry, J. L.
Wainscoat, R. J.
Waterson, M. F.
TI SN 2010ay IS A LUMINOUS AND BROAD-LINED TYPE Ic SUPERNOVA WITHIN A
LOW-METALLICITY HOST GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; supernovae: general; supernovae: individual
(2010ay)
ID GAMMA-RAY BURST; CORE-COLLAPSE SUPERNOVAE; STAR-FORMING GALAXIES;
DIGITAL SKY SURVEY; 25 APRIL 1998; IBC SUPERNOVA; LIGHT CURVES;
100316D/SN 2010BH; PROGENITOR STARS; FORMATION RATES
AB We report on our serendipitous pre-discovery detection and follow-up observations of the broad-lined Type Ic supernova (SN Ic) 2010ay at z = 0.067 imaged by the Pan-STARRS1 3 pi survey just similar to 4 days after explosion. The supernova (SN) had a peak luminosity, M-R approximate to -20.2 mag, significantly more luminous than known GRB-SNe and one of the most luminous SNe Ib/c ever discovered. The absorption velocity of SN 2010ay is v(Si) approximate to 19 x 10(3) km s(-1) at similar to 40 days after explosion, 2-5 times higher than other broad-lined SNe and similar to the GRB-SN 2010bh at comparable epochs. Moreover, the velocity declines similar to 2 times slower than other SNe Ic-BL and GRB-SNe. Assuming that the optical emission is powered by radioactive decay, the peak magnitude implies the synthesis of an unusually large mass of Ni-56, M-Ni = 0.9M(circle dot). Applying scaling relations to the light curve, we estimate a total ejecta mass, M-ej approximate to 4.7 M-circle dot, and total kinetic energy, E-K approximate to 11 x 10(51) erg. The ratio of M-Ni to M-ej is similar to 2 times as large for SN 2010ay as typical GRB-SNe and may suggest an additional energy reservoir. The metallicity (log(O/H)(PP04) + 12 = 8.19) of the explosion site within the host galaxy places SN 2010ay in the low-metallicity regime populated by GRB-SNe, and similar to 0.5(0.2) dex lower than that typically measured for the host environments of normal (broad-lined) SNe Ic. We constrain any gamma-ray emission with E-gamma less than or similar to 6 x 10(48) erg (25-150 keV), and our deep radio follow-up observations with the Expanded Very Large Array rule out relativistic ejecta with energy E greater than or similar to 10(48) erg. We therefore rule out the association of a relativistic outflow like those that accompanied SN 1998bw and traditional long-duration gamma-ray bursts (GRBs), but we place less-stringent constraints on a weak afterglow like that seen from XRF 060218. If this SN did not harbor a GRB, these observations challenge the importance of progenitor metallicity for the production of relativistic ejecta and suggest that other parameters also play a key role.
C1 [Sanders, N. E.; Soderberg, A. M.; Foley, R. J.; Chornock, R.; Chomiuk, L.; Berger, E.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Valenti, S.; Smartt, S.; Botticella, M. T.] Queens Univ Belfast, Astrophys Res Ctr, Sch Maths & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[Chomiuk, L.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Barthelmy, S. D.; Gehrels, N.; Cline, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Levesque, E. M.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA.
[Narayan, G.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Briggs, M. S.; Connaughton, V.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Terada, Y.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan.
[Golenetskii, S.; Mazets, E.] AF Ioffe Phys Tech Inst, Expt Astrophys Lab, St Petersburg 194021, Russia.
[von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Boynton, W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Chambers, K. C.; Heasley, J. N.; Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Kudritzki, R-P.; Luppino, G. A.; Magnier, E. A.; Morgan, J. S.; Onaka, P. M.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ 85919 USA.
[Lupton, R. H.; Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Monet, D. G.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA.
[Waterson, M. F.] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia.
RP Sanders, NE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nsanders@cfa.harvard.edu
RI Terada, Yukikatsu/A-5879-2013; Waterson, Mark/B-7352-2013; Golenetskii,
Sergey/B-3818-2015; Stubbs, Christopher/C-2829-2012
OI Chambers, Kenneth /0000-0001-6965-7789; Terada,
Yukikatsu/0000-0002-2359-1857; Waterson, Mark/0000-0002-0192-2686;
Stubbs, Christopher/0000-0003-0347-1724
FU RFBR [09-02-00166a]; NASA [NNX07AR71G, NNX08AN23G, NNX09AO97G,
NNX08AX95G, NNX09AR28G, NNX09AU03G, NNX09AV61G]; National Aeronautics
and Space Administration through the Planetary Science Division of the
NASA Science Mission Directorate [NNX08AR22G]; National Science
Foundation
FX We are grateful to the following people for their assistance with the
IPN data: C. Meegan (Fermi GBM), K. Yamaoka, M. Ohno, Y. Hanabata, Y.
Fukazawa, T. Takahashi, M. Tashiro, T. Murakami, and K. Makishima
(Suzaku WAM), J. Goldsten (MESSENGER), S. Barthelmy, J. Cummings, H.
Krimm, and D. Palmer (Swift-BAT), R. Aptekar, V. Pal'shin, D. Frederiks,
and D. Svinkin (Konus-Wind), X. Zhang and A. Rau (INTEGRAL SPI-ACS), and
I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin, C. Fellows, K.
Harshman, H. Enos, and R. Starr (Odyssey). The Konus-Wind experiment is
supported in the Russian Federation by RFBR Grant 09-02-00166a. K. H.
acknowledges NASA support for the IPN under the following grants:
NNX07AR71G (MESSENGER), NNX08AN23G and NNX09AO97G (Swift), NNX08AX95G
and NNX09AR28G (INTEGRAL), NNX09AU03G (Fermi), and NNX09AV61G (Suzaku).;
The PS1 Surveys have been made possible through contributions of the
Institute for Astronomy, the University of Hawaii, the Pan-STARRS
Project Office, the Max-Planck Society and its participating institutes,
the Max Planck Institute for Astronomy, Heidelberg and the Max Planck
Institute for Extraterrestrial Physics, Garching, the Johns Hopkins
University, Durham University, the University of Edinburgh, Queen's
University Belfast, the Harvard-Smithsonian Center for Astrophysics, the
Las Cumbres Observatory Global Telescope Network, Incorporated, the
National Central University of Taiwan, and the National Aeronautics and
Space Administration under Grant No. NNX08AR22G issued through the
Planetary Science Division of the NASA Science Mission Directorate.;
This work was supported by the National Science Foundation through a
Graduate Research Fellowship provided to NES.
NR 130
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 184
DI 10.1088/0004-637X/756/2/184
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200080
ER
PT J
AU Smale, AP
Boyd, PT
AF Smale, Alan P.
Boyd, Patricia T.
TI ANOMALOUS LOW STATES AND LONG-TERM VARIABILITY IN THE BLACK HOLE BINARY
LMC X-3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries: close; black hole physics; stars:
individual (LMC X-3); X-rays: binaries
ID X-RAY BINARIES; WARPED ACCRETION DISCS; LARGE-MAGELLANIC-CLOUD; INNER
COOL DISKS; TIMING-EXPLORER; LOW/HARD STATE; MAGNETOROTATIONAL
INSTABILITY; HARD STATE; DISCOVERY; PERIODS
AB Rossi X-ray Timing Explorer observations of the black hole binary LMC X-3 reveal an extended very low X-ray state lasting from 2003 December 13 until 2004 March 18, unprecedented both in terms of its low luminosity (>15 times fainter than ever before seen in this source) and long duration (similar to 3 times longer than a typical low/hard state excursion). During this event little to no source variability is observed on timescales of similar to hours-weeks, and the X-ray spectrum implies an upper limit of 1.2 x 10(35) erg s(-1). Five years later another extended low state occurs, lasting from 2008 December 11 until 2009 June 17. This event lasts nearly twice as long as the first, and while significant variability is observed, the source remains reliably in the low/hard spectral state for the similar to 188 day duration. These episodes share some characteristics with the "anomalous low states" in the neutron star binary Her X-1. The average period and amplitude of the variability of LMC X-3 have different values between these episodes. We characterize the long-term variability of LMC X-3 before and after the two events using conventional and nonlinear time series analysis methods, and show that, as is the case in Her X-1, the characteristic amplitude of the variability is related to its characteristic timescale. Furthermore, the relation is in the same direction in both systems. This suggests that a similar mechanism gives rise to the long-term variability, which in the case of Her X-1 is reliably modeled with a tilted, warped precessing accretion disk.
C1 [Smale, Alan P.; Boyd, Patricia T.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Smale, AP (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM alan.smale@nasa.gov; padi.boyd@nasa.gov
NR 47
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 146
DI 10.1088/0004-637X/756/2/146
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200042
ER
PT J
AU Snyder, GF
Brodwin, M
Mancone, CM
Zeimann, GR
Stanford, SA
Gonzalez, AH
Stern, D
Eisenhardt, PRM
Brown, MJI
Dey, A
Jannuzi, B
Perlmutter, S
AF Snyder, Gregory F.
Brodwin, Mark
Mancone, Conor M.
Zeimann, Gregory R.
Stanford, S. A.
Gonzalez, Anthony H.
Stern, Daniel
Eisenhardt, Peter R. M.
Brown, Michael J. I.
Dey, Arjun
Jannuzi, Buell
Perlmutter, Saul
TI ASSEMBLY OF THE RED SEQUENCE IN INFRARED-SELECTED GALAXY CLUSTERS FROM
THE IRAC SHALLOW CLUSTER SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: elliptical and lenticular, cD;
galaxies: evolution; galaxies: formation; galaxies: photometry
ID COLOR-MAGNITUDE RELATION; HUBBLE-SPACE-TELESCOPE; SIMILAR-TO 1; STELLAR
POPULATION SYNTHESIS; STAR-FORMATION HISTORIES; HIGH-REDSHIFT CLUSTERS;
INITIAL MASS FUNCTION; IA SUPERNOVA RATE; WIDE-FIELD SURVEY; LUMINOSITY
FUNCTION
AB We present results for the assembly and star formation histories (SFHs) of massive (similar to L*) red sequence galaxies (RSGs) in 11 spectroscopically confirmed, infrared-selected galaxy clusters at 1.0 < z < 1.5, the precursors to present-day massive clusters with M similar to 10(15) M-circle dot. Using rest-frame optical photometry, we investigate evolution in the color and scatter of the RSG population, comparing with models of possible SFHs. In contrast to studies of central cluster galaxies at lower redshift (z < 1), these data are clearly inconsistent with the continued evolution of stars formed and assembled primarily at a single, much earlier time. Specifically, we find that the colors of massive cluster galaxies at z approximate to 1.5 imply that the bulk of star formation occurred at z similar to 3, whereas by z approximate to 1 their colors imply formation at z similar to 2; therefore these galaxies exhibit approximately the same luminosity-weighted stellar age at 1 < z < 1.5. This likely reflects star formation that occurs over an extended period, the effects of significant progenitor bias, or both. Our results generally indicate that massive cluster galaxy populations began forming a significant mass of stars at z greater than or similar to 4, contained some red spheroids by z approximate to 1.5, and were actively assembling much of their final mass during 1 < z < 2 in the form of younger stars. Qualitatively, the slopes of the cluster color-magnitude relations are consistent with no significant evolution relative to local clusters.
C1 [Snyder, Gregory F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Mancone, Conor M.; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Zeimann, Gregory R.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Stern, Daniel; Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Dey, Arjun; Jannuzi, Buell] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Perlmutter, Saul] Univ Calif Berkeley, EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Perlmutter, Saul] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
RP Snyder, GF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Brown, Michael/B-1181-2015; Perlmutter, Saul/I-3505-2015
OI Brown, Michael/0000-0002-1207-9137; Perlmutter, Saul/0000-0002-4436-4661
FU NASA [NAS 5-26555]; NASA through grants from the STScI; W.M. Keck
Foundation; NOAO; U.S. Department of Energy [W-7405-ENG-48]; [10496];
[11002]; [11597]; [11663]
FX This work is based on observations made with the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Science Institute (STScI),
which is operated by the Association of Universities for Research in
Astronomy, Inc., (AURA) under NASA contract NAS 5-26555. These
observations are associated with programs 10496, 11002, 11597, and
11663. Support for these programs was provided by NASA through grants
from the STScI, which is operated by AURA under NASA contract NAS
5-26555. This work is also based in part on observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. This work is also 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
NASA. 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. The research activities of A. D. and B.T.J. are also
supported by NOAO, which is operated by the AURA under a cooperative
agreement with the National Science Foundation. MultiDrizzle is a
component of the STSDAS and PyRAF software, products of the STScI, which
is operated by AURA for NASA.; This work relies on considerable efforts
by the Spitzer, HST, and Keck Observatory support staff and instrument
teams, and we thank the many hundreds of people who have contributed to
these facilities over the years. We thank the anonymous referee for a
number of useful suggestions, and Kyle Dawson for a helpful review of
the manuscript. This research has made use of NASA's Astrophysics Data
System. 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 89
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 114
DI 10.1088/0004-637X/756/2/114
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200010
ER
PT J
AU Steffen, JH
Ford, EB
Rowe, JF
Fabrycky, DC
Holman, MJ
Welsh, WF
Batalha, NM
Borucki, WJ
Bryson, S
Caldwell, DA
Ciardi, DR
Jenkins, JM
Kjeldsen, H
Koch, DG
Prsa, A
Sanderfer, DT
Seader, S
Twicken, JD
AF Steffen, Jason H.
Ford, Eric B.
Rowe, Jason F.
Fabrycky, Daniel C.
Holman, Matthew J.
Welsh, William F.
Batalha, Natalie M.
Borucki, William J.
Bryson, Steve
Caldwell, Douglas A.
Ciardi, David R.
Jenkins, Jon M.
Kjeldsen, Hans
Koch, David G.
Prsa, Andrej
Sanderfer, Dwight T.
Seader, Shawn
Twicken, Joseph D.
TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. VI. POTENTIALLY INTERESTING
CANDIDATE SYSTEMS FROM FOURIER-BASED STATISTICAL TESTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: detection; planets and
satellites: dynamical evolution and stability; techniques: miscellaneous
ID MULTIPLE-PLANET SYSTEMS; 1ST 4 MONTHS; TERRESTRIAL PLANETS;
CONFIRMATION; MASS; PERTURBATIONS
AB We analyze the deviations of transit times from a linear ephemeris for the Kepler Objects of Interest (KOI) through quarter six of science data. We conduct two statistical tests for all KOIs and a related statistical test for all pairs of KOIs in multi-transiting systems. These tests identify several systems which show potentially interesting transit timing variations (TTVs). Strong TTV systems have been valuable for the confirmation of planets and their mass measurements. Many of the systems identified in this study should prove fruitful for detailed TTV studies.
C1 [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
[Rowe, Jason F.; Borucki, William J.; Bryson, Steve; Caldwell, Douglas A.; Jenkins, Jon M.; Koch, David G.; Sanderfer, Dwight T.; Seader, Shawn; Twicken, Joseph D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rowe, Jason F.; Caldwell, Douglas A.; Jenkins, Jon M.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA.
[Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500,MS 127, Batavia, IL 60510 USA.
EM jsteffen@fnal.gov
RI Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi,
David/0000-0002-5741-3047; /0000-0001-6545-639X; Fabrycky,
Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [NNX08AR04G, HF-51272.01-A,
HF-51267.01-A, NAS 5-26555]; NASA through Space Telescope Science
Institute
FX Funding for this mission is provided by NASA's Science Mission
Directorate. J.H.S. acknowledges support by NASA under grant NNX08AR04G
issued through the Kepler Participating Scientist Program. D.C.F. and
J.A.C. acknowledge that support for this work was provided by NASA
through Hubble Fellowship grants HF-51272.01-A and HF-51267.01-A awarded
by the Space Telescope Science Institute, operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555.
NR 22
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
IS 2
AR 186
DI 10.1088/0004-637X/756/2/186
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200082
ER
PT J
AU Stritzinger, M
Taddia, F
Fransson, C
Fox, OD
Morrell, N
Phillips, MM
Sollerman, J
Anderson, JP
Boldt, L
Brown, PJ
Campillay, A
Castellon, S
Contreras, C
Folatelli, G
Habergham, SM
Hamuy, M
Hjorth, J
James, PA
Krzeminski, W
Mattila, S
Persson, SE
Roth, M
AF Stritzinger, Maximilian
Taddia, Francesco
Fransson, Claes
Fox, Ori D.
Morrell, Nidia
Phillips, M. M.
Sollerman, Jesper
Anderson, J. P.
Boldt, Luis
Brown, Peter J.
Campillay, Abdo
Castellon, Sergio
Contreras, Carlos
Folatelli, Gaston
Habergham, S. M.
Hamuy, Mario
Hjorth, Jens
James, Phil A.
Krzeminski, Wojtek
Mattila, Seppo
Persson, Sven E.
Roth, Miguel
TI MULTI-WAVELENGTH OBSERVATIONS OF THE ENDURING TYPE IIn SUPERNOVAE 2005ip
AND 2006jd
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: mass-loss; stars: winds, outflows;
supernovae: individual (SN 2005ip, SN 2006jd)
ID VARIABLE CANDIDATE HD-168625; DENSE MASS-LOSS; DUST FORMATION;
CIRCUMSTELLAR INTERACTION; SN 2005IP; INFRARED OBSERVATIONS; LUMINOUS
SUPERNOVAE; RED SUPERGIANTS; STANDARD STARS; IA SUPERNOVA
AB We present an observational study of the Type IIn supernovae (SNe IIn) 2005ip and 2006jd. Broadband UV, optical, and near-IR photometry, and visual-wavelength spectroscopy of SN 2005ip complement and extend upon published observations to 6.5 years past discovery. Our observations of SN 2006jd extend from UV to mid-infrared wavelengths, and like SN 2005ip, are compared to reported X-ray measurements to understand the nature of the progenitor. Both objects display a number of similarities with the 1988Z-like subclass of SN IIn including (1) remarkably similar early-and late-phase optical spectra, (2) a variety of high-ionization coronal lines, (3) long-duration optical and near-IR emission, and (4) evidence of cold and warm dust components. However, diversity is apparent, including an unprecedented late-time r-band excess in SN 2006jd. The observed differences are attributed to differences between the mass-loss history of the progenitor stars. We conclude that the progenitor of SN 2006jd likely experienced a significant mass-loss event during its pre-SN evolution akin to the great 19th century eruption of. Carinae. Contrarily, as advocated by Smith et al., the circumstellar environment of SN 2005ip is found to be more consistent with a clumpy wind progenitor.
C1 [Stritzinger, Maximilian] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Stritzinger, Maximilian; Taddia, Francesco; Fransson, Claes; Sollerman, Jesper] Stockholm Univ, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Fox, Ori D.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Morrell, Nidia; Phillips, M. M.; Campillay, Abdo; Castellon, Sergio; Contreras, Carlos; Krzeminski, Wojtek; Roth, Miguel] Las Campanas Observ, Carnegie Observ, La Serena, Chile.
[Anderson, J. P.; Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile.
[Boldt, Luis] Univ Bonn, Argelander Inst Astron, D-53111 Bonn, Germany.
[Brown, Peter J.] Texas A&M Univ, Mitchell Inst Fundamental Phys & Astron, Dept Phys & Astron, College Stn, TX 77843 USA.
[Folatelli, Gaston] Univ Tokyo, IPMU, Kashiwa, Chiba 2778583, Japan.
[Habergham, S. M.; James, Phil A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Hjorth, Jens] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Mattila, Seppo] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland.
[Persson, Sven E.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
RP Stritzinger, M (reprint author), Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
RI Hjorth, Jens/M-5787-2014; Hamuy, Mario/G-7541-2016;
OI Hjorth, Jens/0000-0002-4571-2306; Sollerman, Jesper/0000-0003-1546-6615;
James, Philip/0000-0003-4131-5183; stritzinger,
maximilian/0000-0002-5571-1833
FU NSF [AST-0306969, AST-0607438, AST-1008343]; Swedish Research Council;
Swedish National Space Board; NASA; CONICYT through FONDECYT [3110142];
Millennium Center for Supernova Science [P10-064-F]; Danish National
Research Foundation; National Aeronautics and Space Administration
FX We thank Jose-Luis Prieto for calling to our attention the WISE
observations of SN 2006jd. This material is based upon work supported by
NSF under grants AST-0306969, AST-0607438, and AST-1008343. The Oskar
Klein Centre is funded by the Swedish Research Council. C. F.
acknowledges support from the Swedish Research Council and the Swedish
National Space Board. O.D.F. thanks the NASA Postdoctoral Program
fellowship for support. J.P.A. and M. H. acknowledge support by CONICYT
through FONDECYT grant 3110142, and the Millennium Center for Supernova
Science (P10-064-F). The Dark Cosmology Centre is funded by the Danish
National Research Foundation. The Isaac Newton Telescope is operated on
the island of La Palma by the Isaac Newton Group in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias. Also 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 of the Instituto de Astrofisica de Canarias. 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 85
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
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VL 756
IS 2
AR 173
DI 10.1088/0004-637X/756/2/173
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200069
ER
PT J
AU van Engelen, A
Keisler, R
Zahn, O
Aird, KA
Benson, BA
Bleem, LE
Carlstrom, E
Chang, CL
Cho, HM
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Dudley, J
George, EM
Halverson, NW
Holder, GP
Holzapfel, WL
Hoover, S
Hou, Z
Hrubes, D
Joy, M
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
McMahon, JJ
Mehl, J
Meyer, SS
Millea, M
Mohr, JJ
Montroy, TE
Natoli, T
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Ruhl, JE
Sayre, JT
Schaffer, KK
Shaw, L
Shirokoff, E
Spieler, HG
Staniszewski, Z
Stark, AA
Story, K
Vanderlinde, K
Vieira, JD
Williamson, R
AF van Engelen, A.
Keisler, R.
Zahn, O.
Aird, K. A.
Benson, B. A.
Bleem, L. E.
Carlstrom, E.
Chang, C. L.
Cho, H. M.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Dudley, J.
George, E. M.
Halverson, N. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hou, Z.
Hrubes, D.
Joy, M.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Millea, M.
Mohr, J. J.
Montroy, T. E.
Natoli, T.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Ruhl, J. E.
Sayre, J. T.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Spieler, H. G.
Staniszewski, Z.
Stark, A. A.
Story, K.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
TI A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING
SOUTH POLE TELESCOPE DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology:
observations; gravitational lensing: weak; large-scale structure of
universe
ID ATACAMA COSMOLOGY TELESCOPE; PROBE WMAP OBSERVATIONS; POWER SPECTRUM;
GALAXY CLUSTERS; EXTRAGALACTIC SOURCES; DARK-MATTER; DAMPING TAIL; 148
GHZ; CMB; ANISOTROPIES
AB We use South Pole Telescope data from 2008 and 2009 to detect the non-Gaussian signature in the cosmic microwave background (CMB) produced by gravitational lensing and to measure the power spectrum of the projected gravitational potential. We constrain the ratio of the measured amplitude of the lensing signal to that expected in a fiducial Lambda CDM cosmological model to be 0.86 +/- 0.16, with no lensing disfavored at 6.3 sigma. Marginalizing over Lambda CDM cosmological models allowed by the Wilkinson Microwave Anisotropy Probe (WMAP7) results in a measurement of A(lens) = 0.90 +/- 0.19, indicating that the amplitude of matter fluctuations over the redshift range 0.5 less than or similar to z less than or similar to 5 probed by CMB lensing is in good agreement with predictions. We present the results of several consistency checks. These include a clear detection of the lensing signature in CMB maps filtered to have no overlap in Fourier space, as well as a "curl" diagnostic that is consistent with the signal expected for Lambda CDM. We perform a detailed study of bias in the measurement due to noise, foregrounds, and other effects and determine that these contributions are relatively small compared to the statistical uncertainty in the measurement. We combine this lensing measurement with results from WMAP7 to improve constraints on cosmological parameters when compared to those from WMAP7 alone: we find a factor of 3.9 improvement in the measurement of the spatial curvature of the universe, Omega(k) = -0.0014 +/- 0.0172; a 10% improvement in the amplitude of matter fluctuations within Lambda CDM, sigma(8) = 0.810 +/- 0.026; and a 5% improvement in the dark energy equation of state, w = -1.04 +/- 0.40. When compared with the measurement of w provided by the combination of WMAP7 and external constraints on the Hubble parameter, the addition of the lensing data improves the measurement of w by 15% to give w = -1.087 +/- 0.096.
C1 [van Engelen, A.; de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Keisler, R.; Benson, B. A.; Bleem, L. E.; Carlstrom, E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Keisler, R.; Bleem, L. E.; Carlstrom, E.; Hoover, S.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
[Benson, B. A.; Carlstrom, E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Carlstrom, E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cho, H. M.; Shirokoff, E.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Joy, M.] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP van Engelen, A (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; Stark,
Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics
Frontier Center at the University of Chicago [0114422]; Kavli
Foundation; Gordon and Betty Moore Foundation; National Sciences and
Engineering Research Council of Canada; Canada Research Chairs program;
Canadian Institute for Advanced Research; Inaugural Berkeley Center for
Cosmological Physics Fellowship; NASA Hubble Fellowship [HF-51275.01];
KICP Fellowship; Alfred P. Sloan Research Fellowship; Yale University;
NSF [AST-1009811]; Excellence Cluster Universe; DFG research program
[TR33]; Office of Science of the U.S. Department of Energy
[DE-AC02-05CH11231]; NASA Office of Space Science
FX The South Pole Telescope is supported by the National Science Foundation
through grants ANT-0638937 and ANT-0130612. Partial support is also
provided by the NSF Physics Frontier Center grant PHY-0114422 to the
Kavli Institute of Cosmological Physics at the University of Chicago,
the Kavli Foundation and the Gordon and Betty Moore Foundation. The
McGill group acknowledges funding from the National Sciences and
Engineering Research Council of Canada, Canada Research Chairs program,
and the Canadian Institute for Advanced Research. Oliver Zahn
acknowledges support from an Inaugural Berkeley Center for Cosmological
Physics Fellowship. R. Keisler acknowledges support from the NASA Hubble
Fellowship grant HF-51275.01. B. A. Benson is supported by a KICP
Fellowship. M. Dobbs acknowledges support from an Alfred P. Sloan
Research Fellowship. L. Shaw acknowledges the support of Yale University
and the NSF grant AST-1009811. M. Millea and L. Knox acknowledge the
support of the NSF grant 0709498. J. Mohr acknowledges support from the
Excellence Cluster Universe and the DFG research program TR33 "Dark
Universe." This research used resources of the National Energy Research
Scientific Computing Center, which is supported by the Office of Science
of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.
It also used resources of the CLUMEQ supercomputing consortium, part of
the Compute Canada network. 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. Some of the results in
this paper have been derived using the HEALPix (Gorski et al. 2005)
package.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200038
ER
PT J
AU Wolff, CL
AF Wolff, Charles L.
TI ARE PULSING SOLITARY WAVES RUNNING INSIDE THE SUN?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE hydrodynamics; Sun: interior; Sun: oscillations; waves
ID NEUTRINO CAPTURE RATE; SOLAR G-MODES; GLOBAL OSCILLATIONS; SPECTRUM
ANALYSIS; CORE; FLUX; PULSATIONS; STABILITY; ROTATION; CYCLES
AB A precise sequence of frequencies-detected four independent ways-is interpreted as a system of solitary waves below the Sun's convective envelope. Six future observational or theoretical tests of this idea are suggested. Wave properties (rotation rates, radial energy distribution, nuclear excitation strength) follow from conventional dynamics of global oscillation modes after assuming a localized nuclear term strong enough to perturb and hold mode longitudes into alignments that form "families." To facilitate future tests, more details are derived for a system of two dozen solitary waves 2 <= l <= 25. Wave excitation by He-3 and C-14 burning is complex. It spikes by factors M-1 <= 10(3) when many waves overlap in longitude but its long-time average is M-2 <= 10. Including mixing can raise overall excitation to similar to 50 times that in a standard solar model. These spikes cause tiny phase shifts that tend to pull wave rotation rates toward their ideal values. alpha[l(l + 1)](-1). A system like this would generate some extra nuclear energy in two spots at low latitude on opposite sides of the Sun. Each covers about 20 degrees of longitude. Above a certain wave amplitude, the system starts giving distinctly more nuclear excitation to some waves (e. g., l = 9, 14, and 20) than to neighboring l values. The prominence of l = 20 has already been reported. This transition begins at temperature amplitudes Delta T/T = 0.03 in the solar core for a typical family of modes, which corresponds to delta T/T similar to 0.001 for one of its many component oscillation modes.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wolff, CL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM charles.l.wolff@nasa.gov
OI Wolff, Charles/0000-0001-8854-507X
FU Heliophysics Science Division of Goddard Space Flight Center
FX I appreciate support of this publication by the Heliophysics Science
Division of Goddard Space Flight Center.
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SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
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SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200021
ER
PT J
AU Zeimann, GR
Stanford, SA
Brodwin, M
Gonzalez, AH
Snyder, GF
Stern, D
Eisenhardt, P
Mancone, C
Dey, A
AF Zeimann, Gregory R.
Stanford, S. A.
Brodwin, Mark
Gonzalez, Anthony H.
Snyder, Gregory F.
Stern, Daniel
Eisenhardt, Peter
Mancone, Conor
Dey, Arjun
TI IDCS J1433.2+3306: AN INFRARED-SELECTED GALAXY CLUSTER AT z=1.89
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (IDCS J1433.2+3306); galaxies: distances
and redshifts; galaxies: evolution; galaxies: formation; galaxies:
photometry; galaxies: star formation
ID ACTIVE GALACTIC NUCLEI; IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY; X-RAY
SURVEY; STAR-FORMATION; RED-SEQUENCE; DEEP; CONFIRMATION; EXTRACTION;
RESOLUTION
AB We report the discovery of an IR-selected galaxy cluster in the IRAC Distant Cluster Survey (IDCS). New data from the Hubble Space Telescope spectroscopically confirm IDCS J1433.2+3306 at z = 1.89 with robust spectroscopic redshifts for seven members, two of which are based on the 4000 angstrom break. Detected emission lines such as [O II] and H beta indicate star formation rates of greater than or similar to 20 M-circle dot yr(-1) for three galaxies within a 500 kpc projected radius of the cluster center. The cluster exhibits a red sequence with a scatter and color indicative of a formation redshift z(f) greater than or similar to 3.5. The stellar age of the early-type galaxy population is approximately consistent with those of clusters at lower redshift (1 < z < 1.5) suggesting that clusters at these redshifts are experiencing ongoing or increasing star formation.
C1 [Zeimann, Gregory R.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA.
[Gonzalez, Anthony H.; Mancone, Conor] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Snyder, Gregory F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stern, Daniel; Eisenhardt, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Zeimann, GR (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA.
FU National Science Foundation [AST-0708490]; NASA through JPL/Caltech;
NASA from the Space Telescope Science Institute [11663, 12203]; NASA
[NAS 5-26555]; W. M. Keck Foundation; U.S. Department of Energy
[W-7405-ENG-48]
FX 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 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 NASA contract NAS 5-26555. 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. 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 the anonymous referee for their constructive comments, 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,
and Steve Murray and the XBootes team for obtaining the Chandra data in
the Bootes field. This paper would not have been possible without the
efforts of the support staff of the Keck Observatory, Spitzer Space
Telescope, Hubble Space Telescope, and Chandra X-ray Observatory. 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.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2012
VL 756
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AR 115
DI 10.1088/0004-637X/756/2/115
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200011
ER
PT J
AU Zhang, BB
Fan, YZ
Shen, RF
Xu, D
Zhang, FW
Wei, DM
Burrows, DN
Zhang, B
Gehrels, N
AF Zhang, Bin-Bin
Fan, Yi-Zhong
Shen, Rong-Feng
Xu, Dong
Zhang, Fu-Wen
Wei, Da-Ming
Burrows, David N.
Zhang, Bing
Gehrels, Neil
TI GRB 120422A: A LOW-LUMINOSITY GAMMA-RAY BURST DRIVEN BY A CENTRAL ENGINE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; X-rays: general
ID AFTERGLOW LIGHT CURVES; SHOCK BREAKOUT; LORENTZ-FACTOR; SPECTRAL
EVOLUTION; RELATIVISTIC JETS; PROMPT EMISSION; SUPERNOVA; GRB-060218;
LONG; TELESCOPE
AB GRB 120422A is a low-luminosity gamma-ray burst (GRB) associated with a bright supernova, which distinguishes itself by its relatively short T-90 (similar to 5 s) and an energetic and steep-decaying X-ray tail. We analyze the Swift Burst Alert Telescope and X-ray Telescope data and discuss the physical implications. We show that the steep decline early in the X-ray light curve can be interpreted as the curvature tail of a late emission episode around 58-86 s, with a curved instantaneous spectrum at the end of the emission episode. Together with the main activity in the first similar to 20 s and the weak emission from 40 s to 60 s, the prompt emission is variable, which points to a central engine origin in contrast to a shock-breakout origin, which is used to interpret some other nearby low-luminosity supernova GRBs. Both the curvature effect model and interpreting the early shallow decay as the coasting external forward shock emission in a wind medium provide a constraint on the bulk Lorentz factor Gamma to be around several. Comparing the properties of GRB 120422A and other supernova GRBs, we find that the main criterion to distinguish engine-driven GRBs from shock-breakout GRBs is the time-averaged gamma-ray luminosity. Engine-driven GRBs likely have a luminosity above similar to 10(48) erg s(-1).
C1 [Zhang, Bin-Bin; Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Fan, Yi-Zhong; Wei, Da-Ming] Nanjing Univ, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China.
[Fan, Yi-Zhong; Wei, Da-Ming] Chinese Acad Sci, Key Lab Dark Matter & Space Astron, Nanjing 210008, Jiangsu, Peoples R China.
[Shen, Rong-Feng] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Xu, Dong] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, IL-76100 Rehovot, Israel.
[Xu, Dong] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Zhang, Fu-Wen] Guilin Univ Technol, Coll Sci, Guilin 541004, Guangxi, Peoples R China.
[Zhang, Bing] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhang, BB (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM bbzhang@psu.edu; yzfan@pmo.ac.cn; zhang@physics.unlv.edu
RI Zhang, Binbin/C-9035-2013
OI Zhang, Binbin/0000-0003-2002-116X
FU NASA SAO [SV4-74018]; National Natural Science Foundation of China
[10973041, 10921063, 11073057, 11163003]; National Basic Research
Program of China [2009CB824800]; Chinese Academy of Sciences; NASA
[NNX10AD08G]; NSF [AST-0908362]
FX We thank Derek B. Fox, Peter Meszaros, Dirk Grupe, and Peter Veres for
helpful discussions. This work is supported in part by NASA SAO
SV4-74018 (B.B.Z.), the National Natural Science Foundation of China
(grants 10973041, 10921063, 11073057, and 11163003) and the National
Basic Research Program of China under grant 2009CB824800, the 100
Talents Program of Chinese Academy of Sciences (Y.Z.F.), NASA
NNX10AD08G, and NSF AST-0908362 (B.Z.).
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
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PG 6
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SC Astronomy & Astrophysics
GA 009TN
UT WOS:000309048200086
ER
PT J
AU Cliver, EW
Ling, AG
Belov, A
Yashiro, S
AF Cliver, E. W.
Ling, A. G.
Belov, A.
Yashiro, S.
TI SIZE DISTRIBUTIONS OF SOLAR FLARES AND SOLAR ENERGETIC PARTICLE EVENTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: flares; Sun: particle emission; Sun: coronal mass ejections (CMEs);
Sun: X-rays, gamma-rays
ID CORONAL MASS EJECTIONS; II RADIO-BURSTS; X-RAY FLARES; PROTON EVENTS;
FREQUENCY-DISTRIBUTIONS; PARAMETERS; SPECTRA; ACCELERATION; FLUXES;
CYCLES
AB We suggest that the flatter size distribution of solar energetic proton (SEP) events relative to that of flare soft X-ray (SXR) events is primarily due to the fact that SEP flares are an energetic subset of all flares. Flares associated with gradual SEP events are characteristically accompanied by fast (>= 1000 km s(-1)) coronal mass ejections (CMEs) that drive coronal/interplanetary shock waves. For the 1996-2005 interval, the slopes (alpha values) of power-law size distributions of the peak 1-8 angstrom fluxes of SXR flares associated with (a) >10 MeV SEP events (with peak fluxes >= 1 pr cm(-2) s(-1) sr(-1)) and (b) fast CMEs were similar to 1.3-1.4 compared to similar to 1.2 for the peak proton fluxes of >10 MeV SEP events and similar to 2 for the peak 1-8 angstrom fluxes of all SXR flares. The difference of similar to 0.15 between the slopes of the distributions of SEP events and SEP SXR flares is consistent with the observed variation of SEP event peak flux with SXR peak flux.
C1 [Cliver, E. W.] USAF, Res Lab, Space Vehicles Directorate, Sunspot, NM 88349 USA.
[Ling, A. G.] Atmospher Environm Res, Lexington, MA 02421 USA.
[Belov, A.] IZMIRAN, Troitsk 142190, Moscow Region, Russia.
[Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yashiro, S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Cliver, EW (reprint author), USAF, Res Lab, Space Vehicles Directorate, Sunspot, NM 88349 USA.
FU AFOSR Task [2301RDZ4]; AFRL contract [FA8718-05-C-0036]
FX E.W.C. thanks Karel Schrijver and Jurg Beer for organizing a series of
stimulating ISSI workshops on Extreme Solar Events. We thank Hugh Hudson
and Karel Schrijver for helpful comments on the manuscript. E.W.C. was
supported under AFOSR Task 2301RDZ4 and A.G.L. acknowledges support from
AFRL contract FA8718-05-C-0036.
NR 31
TC 19
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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 SEP 10
PY 2012
VL 756
IS 2
AR L29
DI 10.1088/2041-8205/756/2/L29
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 006CH
UT WOS:000308796500005
ER
PT J
AU Huenemoerder, DP
Oskinova, LM
Ignace, R
Waldron, WL
Todt, H
Hamaguchi, K
Kitamoto, S
AF Huenemoerder, David P.
Oskinova, Lidia M.
Ignace, Richard
Waldron, Wayne L.
Todt, Helge
Hamaguchi, Kenji
Kitamoto, Shunji
TI ON THE WEAK-WIND PROBLEM IN MASSIVE STARS: X-RAY SPECTRA REVEAL A
MASSIVE HOT WIND IN mu COLUMBAE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: early-type; stars: individual (mu Col); stars: mass-loss; X-rays:
stars
ID BLANKETED MODEL ATMOSPHERES; SEQUENCE B-STARS; O-TYPE STARS; STELLAR
WIND; LINE INTENSITIES; EMISSION; SPECTROSCOPY; PLASMA; MOMENTUM;
ORIONIS
AB mu Columbae is a prototypical weak-wind O star for which we have obtained a high-resolution X-ray spectrum with the Chandra LETG/ACIS instrument and a low-resolution spectrum with Suzaku. This allows us, for the first time, to investigate the role of X-rays on the wind structure in a bona fide weak-wind system and to determine whether there actually is a massive hot wind. The X-ray emission measure indicates that the outflow is an order of magnitude greater than that derived from UV lines and is commensurate with the nominal wind-luminosity relationship for O stars. Therefore, the "weak-wind problem"-identified from cool wind UV/optical spectra-is largely resolved by accounting for the hot wind seen in X-rays. From X-ray line profiles, Doppler shifts, and relative strengths, we find that this weak-wind star is typical of other late O dwarfs. The X-ray spectra do not suggest a magnetically confined plasma-the spectrum is soft and lines are broadened; Suzaku spectra confirm the lack of emission above 2 keV. Nor do the relative line shifts and widths suggest any wind decoupling by ions. The He-like triplets indicate that the bulk of the X-ray emission is formed rather close to the star, within five stellar radii. Our results challenge the idea that some OB stars are "weak-wind" stars that deviate from the standard wind-luminosity relationship. The wind is not weak, but it is hot and its bulk is only detectable in X-rays.
C1 [Huenemoerder, David P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Oskinova, Lidia M.; Todt, Helge] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Ignace, Richard] E Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA.
[Waldron, Wayne L.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Hamaguchi, Kenji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Hamaguchi, Kenji] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Hamaguchi, Kenji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Kitamoto, Shunji] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan.
RP Huenemoerder, DP (reprint author), MIT, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA.
RI XRAY, SUZAKU/A-1808-2009
FU National Aeronautics and Space Administration through Chandra Award
[GO1-12017A, GO1-12017B, GO1-12017C]; National Aeronautics Space
Administration [NAS8-03060]; DLR grant [FKZ 50 OR 1101]
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Numbers GO1-12017A (WLW),
GO1-12017B (DPH), and GO1-12017C (RI) issued by the Chandra X-ray
Observatory Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics Space
Administration under contract NAS8-03060. L.M.O. was funded by DLR grant
FKZ 50 OR 1101. We thank W.-R. Hamann for comments and help with PoWR
code.
NR 40
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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 SEP 10
PY 2012
VL 756
IS 2
AR L34
DI 10.1088/2041-8205/756/2/L34
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 006CH
UT WOS:000308796500010
ER
PT J
AU Paganini, L
Mumma, MJ
Villanueva, GL
DiSanti, MA
Bonev, BP
Lippi, M
Boehnhardt, H
AF Paganini, L.
Mumma, M. J.
Villanueva, G. L.
DiSanti, M. A.
Bonev, B. P.
Lippi, M.
Boehnhardt, H.
TI THE CHEMICAL COMPOSITION OF CO-RICH COMET C/2009 P1 (GARRADD) AT R-h =
2.4 AND 2.0 AU BEFORE PERIHELION (vol 748, L13, 2012)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Correction
C1 [Paganini, L.; Mumma, M. J.; Villanueva, G. L.; DiSanti, M. A.; Bonev, B. P.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Villanueva, G. L.; Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Lippi, M.; Boehnhardt, H.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
RP Paganini, L (reprint author), NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, MS 690, Greenbelt, MD 20771 USA.
EM lucas.paganini@nasa.gov
RI mumma, michael/I-2764-2013
NR 1
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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 SEP 10
PY 2012
VL 756
IS 2
AR L42
DI 10.1088/2041-8205/756/2/L42
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 006CH
UT WOS:000308796500018
ER
PT J
AU Su, Y
Wang, TJ
Veronig, A
Temmer, M
Gan, WQ
AF Su, Yang
Wang, Tongjiang
Veronig, Astrid
Temmer, Manuela
Gan, Weiqun
TI SOLAR MAGNETIZED "TORNADOES:" RELATION TO FILAMENTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences; Sun: surface magnetism; Sun:
UV radiation
ID PROMINENCES; NETWORK; CAVITY; FIELDS; DYNAMICS; FLOWS; SUN
AB Solar magnetized "tornadoes," a phenomenon discovered in the solar atmosphere, appear as tornado-like structures in the corona but are rooted in the photosphere. Like other solar phenomena, solar tornadoes are a feature of magnetized plasma and therefore differ distinctly from terrestrial tornadoes. Here we report the first analysis of solar "tornadoes" (two papers which focused on different aspects of solar tornadoes were published in the Astrophysical Journal Letters and Nature, respectively, during the revision of this Letter). A detailed case study of two events indicates that they are rotating vertical magnetic structures probably driven by underlying vortex flows in the photosphere. They usually exist as a group and are related to filaments/prominences, another important solar phenomenon whose formation and eruption are still mysteries. Solar tornadoes may play a distinct role in the supply of mass and twists to filaments. These findings could lead to a new explanation of filament formation and eruption.
C1 [Su, Yang; Veronig, Astrid; Temmer, Manuela] Graz Univ, IGAM Kanzelhohe Observ, Inst Phys, A-8010 Graz, Austria.
[Wang, Tongjiang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wang, Tongjiang] NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Gan, Weiqun] Chinese Acad Sci, Key Lab Dark Matter & Space Astron, Purple Mt Observ, Nanjing 210008, Peoples R China.
RP Su, Y (reprint author), Graz Univ, IGAM Kanzelhohe Observ, Inst Phys, Univ Pl 5, A-8010 Graz, Austria.
EM yang.su@uni-graz.at
RI Veronig, Astrid/B-8422-2009; Su, Yang/J-5381-2014;
OI Temmer, Manuela/0000-0003-4867-7558
FU European Community Framework Programme 7, High Energy Solar Physics Data
in Europe (HESPE) [263086]; NASA grants [NNX10AN10G, NNX12AB34G]
FX We thank the referee for the valuable comments. The space observations
used in this study were obtained from the Solar Dynamics Observatory
(SDO) and the Solar Terrestrial Relations Observatory (STEREO). SDO is a
mission for NASA's Living With a Star (LWS) Program. The ground
observations were obtained from the National Solar Observatory-GONG, the
Observatory of Paris-Meudon in France, and the Kanzelhohe Observatory
(KSO)/University of Graz in Austria. This work utilizes data obtained by
the Global Oscillation Network Group (GONG) Program, managed by the
National Solar Observatory, which is operated by AURA, Inc. under a
cooperative agreement with the National Science Foundation. The data
were acquired by instruments operated by the Big Bear Solar Observatory,
High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar
Observatory, Instituto de Astrofisica de Canarias, and Cerro Tololo
Interamerican Observatory. This activity has been supported by the
European Community Framework Programme 7, High Energy Solar Physics Data
in Europe (HESPE), grant agreement No. 263086. The work of T.W. was
supported by NASA grants NNX10AN10G and NNX12AB34G. M.T. greatly
acknowledges the Austrian Science Fund (FWF): FWF V195-N16. W.G.
acknowledges 2011CB811402 by MSTC.
NR 30
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U1 2
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 10
PY 2012
VL 756
IS 2
AR L41
DI 10.1088/2041-8205/756/2/L41
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 006CH
UT WOS:000308796500017
ER
PT J
AU Sauer, MJ
Roesler, CS
Werdell, PJ
Barnard, A
AF Sauer, Michael J.
Roesler, C. S.
Werdell, P. J.
Barnard, A.
TI Under the hood of satellite empirical chlorophyll a algorithms:
revealing the dependencies of maximum band ratio algorithms on inherent
optical properties
SO OPTICS EXPRESS
LA English
DT Article
ID DISSOLVED ORGANIC-MATTER; CASE-I WATERS; OCEAN COLOR;
MARINE-PHYTOPLANKTON; LIGHT-SCATTERING; CASE-1 WATERS; TIME-SERIES;
ABSORPTION; VARIABILITY; PARTICLES
AB Empirically-based satellite estimates of chlorophyll a [Chl] (e.g. OC3) are an important indicator of phytoplankton biomass. To correctly interpret [Chl] variability, estimates must be accurate and sources of algorithm errors known. While the underlying assumptions of band ratio algorithms such as OC3 have been tacitly hypothesized (i.e. CDOM and phytoplankton absorption covary), the influence of component absorption and scattering on the shape of the algorithm and estimated [Chl] error has yet to be explicitly revealed. We utilized the NOMAD bio-optical data set to examine variations between satellite estimated [Chl] and in situ values. We partitioned the variability into (a) signal contamination and (b) natural phytoplankton variability (variability in chlorophyll-specific phytoplankton absorption). Not surprisingly, the OC3 best-fit curve resulted from a balance between these two different sources of variation confirming the bias by detrital absorption on global scale. Unlike previous descriptions of empirical [Chl] algorithms, our study (a) quantified the mean detrital: phytoplankton absorption as similar to 1:1in the global NOMAD data set, and (b) removed detrital (CDOM + non-algal particle) absorption in radiative transfer models directly showing that the scale of the remaining variability in the band ratio algorithm was dominated by phytoplankton absorption cross section. (C) 2012 Optical Society of America
C1 [Sauer, Michael J.] US Geol Survey, Sacramento, CA 95819 USA.
[Roesler, C. S.] Bowdoin Coll, Dept Earth & Oceanog Sci, Brunswick, ME 04011 USA.
[Werdell, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sauer, MJ (reprint author), US Geol Survey, 6000 J St,Placer Hall, Sacramento, CA 95819 USA.
EM msauer@usgs.gov
FU NASA [NNX08AU83H]
FX This work was funded by NASA Earth Space Fellowship #NNX08AU83H to MJS.
The authors wish to thank three anonymous reviewers for their helpful
comments and advice on this manuscript.
NR 48
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PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD SEP 10
PY 2012
VL 20
IS 19
BP 20920
EP 20933
DI 10.1364/OE.20.020920
PG 14
WC Optics
SC Optics
GA 007CE
UT WOS:000308865600036
PM 23037216
ER
PT J
AU Sun, XL
Abshire, JB
AF Sun, Xiaoli
Abshire, James B.
TI Comparison of IPDA lidar receiver sensitivity for coherent detection and
for direct detection using sine-wave and pulsed modulation
SO OPTICS EXPRESS
LA English
DT Article
ID LASER-ABSORPTION SPECTROMETER; BOUNDARY-LAYER; MIXING-RATIO; CO2 LIDAR
AB We use theoretical models to compare the receiver signal to noise ratio (SNR) vs. average rate of detected signal photons for an integrated path differential absorption (IPDA) lidar using coherent detection with continuous wave (CW) lasers and direct detection with sine-wave and pulse modulations. The results show the coherent IPDA lidar has high receiver gain and narrow bandwidth to overcome the effects of detector circuit noise and background light, but the actual receiver performance can be limited by the coherent mixing efficiency, speckle and other factors. For direct detection, using sine-wave modulation allows the use of a low peak power laser transmitter and synchronous detection. The pulse modulation technique requires higher laser peak powers but is more efficient than sine-wave modulation in terms of average detected signal photon rate required to achieve a given receiver SNR. We also conducted experiments for the direct detection cases and the results agreed well with theory. (C) 2012 Optical Society of America
C1 [Sun, Xiaoli; Abshire, James B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sun, XL (reprint author), NASA, Goddard Space Flight Ctr, Code 690, Greenbelt, MD 20771 USA.
EM xiaoli.sun-1@nasa.gov
RI Sun, Xiaoli/B-5120-2013; Abshire, James/I-2800-2013
FU NASA Earth Science Technology Office (ESTO) Instrument Incubator Program
(IIP)
FX This work was supported by the NASA Earth Science Technology Office
(ESTO) Instrument Incubator Program (IIP). We appreciate the helpful
suggestions by the reviewers.
NR 17
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U1 4
U2 21
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD SEP 10
PY 2012
VL 20
IS 19
BP 21291
EP 21304
DI 10.1364/OE.20.021291
PG 14
WC Optics
SC Optics
GA 007CE
UT WOS:000308865600071
PM 23037252
ER
PT J
AU Lin, GP
Furst, J
Strekalov, DV
Grudinin, IS
Yu, N
AF Lin, Guoping
Fuerst, Josef
Strekalov, Dmitry V.
Grudinin, Ivan S.
Yu, Nan
TI High-Q UV whispering gallery mode resonators made of angle-cut BBO
crystals
SO OPTICS EXPRESS
LA English
DT Article
ID GENERATION; EMISSION
AB We report an investigation on angle-cut beta barium borate (BBO) whispering gallery mode (WGM) resonators operating in the ultra violet (UV) wavelength range. A quality (Q) factor of 1.5 x 10(8) has been demonstrated at 370 nm. New upper bounds for the absorption coefficients of BBO are obtained from the Q factor measurements. Moreover, polarization rotations of WGMs in the angle-cut birefringent resonators are observed and investigated. To the best of our knowledge, this is not only the first reported demonstration of an angle-cut WGM resonator but also the first reported high Q WGM resonator in the UV region. (C) 2012 Optical Society of America
C1 [Lin, Guoping; Fuerst, Josef; Strekalov, Dmitry V.; Grudinin, Ivan S.; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fuerst, Josef] Univ Erlangen Nurnberg, Inst Opt Informat & Photon, D-91058 Erlangen, Germany.
RP Lin, GP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nan.yu@jpl.nasa.gov
RI Lin, Guoping/I-3381-2015
OI Lin, Guoping/0000-0003-4007-1850
FU NASA; Max Planck Society
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA. We acknowledge
discussions with Doctor Harald Schwefel and Florian Sedlmeir. G. Lin
acknowledges support from the NASA Postdoctoral Program, administered by
Oak Ridge Associated Universities (ORAU). J. Furst acknowledges
financial support from the Max Planck Society.
NR 14
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PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD SEP 10
PY 2012
VL 20
IS 19
BP 21372
EP 21378
DI 10.1364/OE.20.021372
PG 7
WC Optics
SC Optics
GA 007CE
UT WOS:000308865600079
PM 23037260
ER
PT J
AU Knobelspiesse, K
Cairns, B
Mishchenko, M
Chowdhary, J
Tsigaridis, K
van Diedenhoven, B
Martin, W
Ottaviani, M
Alexandrov, M
AF Knobelspiesse, Kirk
Cairns, Brian
Mishchenko, Michael
Chowdhary, Jacek
Tsigaridis, Kostas
van Diedenhoven, Bastiaan
Martin, William
Ottaviani, Matteo
Alexandrov, Mikhail
TI Analysis of fine-mode aerosol retrieval capabilities by different
passive remote sensing instrument designs
SO OPTICS EXPRESS
LA English
DT Article
ID IMAGING SPECTRORADIOMETER MISR; UNIFIED SATELLITE CLIMATOLOGY;
OPTICAL-THICKNESS; PHOTOPOLARIMETRIC MEASUREMENTS; PLANETARY
ATMOSPHERES; POLARIZED REFLECTANCE; CLOUD PROPERTIES; A-TRAIN;
MULTIANGLE; AERONET
AB Remote sensing of aerosol optical properties is difficult, but multi-angle, multi-spectral, polarimetric instruments have the potential to retrieve sufficient information about aerosols that they can be used to improve global climate models. However, the complexity of these instruments means that it is difficult to intuitively understand the relationship between instrument design and retrieval success. We apply a Bayesian statistical technique that relates instrument characteristics to the information contained in an observation. Using realistic simulations of fine size mode dominated spherical aerosols, we investigate three instrument designs. Two of these represent instruments currently in orbit: the Multiangle Imaging SpectroRadiometer (MISR) and the POLarization and Directionality of the Earths Reflectances (POLDER). The third is the Aerosol Polarimetry Sensor (APS), which failed to reach orbit during recent launch, but represents a viable design for future instruments. The results show fundamental differences between the three, and offer suggestions for future instrument design and the optimal retrieval strategy for current instruments. Generally, our results agree with previous validation efforts of POLDER and airborne prototypes of APS, but show that the MISR aerosol optical thickness uncertainty characterization is possibly underestimated. (C) 2012 Optical Society of America
C1 [Knobelspiesse, Kirk; Cairns, Brian; Mishchenko, Michael; Chowdhary, Jacek; Tsigaridis, Kostas; van Diedenhoven, Bastiaan; Martin, William; Ottaviani, Matteo; Alexandrov, Mikhail] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Knobelspiesse, Kirk] NASA, Postdoctoral Program, Washington, DC USA.
[Chowdhary, Jacek; Tsigaridis, Kostas; van Diedenhoven, Bastiaan; Martin, William; Alexandrov, Mikhail] Columbia Univ, New York, NY 10025 USA.
[Ottaviani, Matteo] Stevens Inst Technol, Hoboken, NJ 07030 USA.
RP Knobelspiesse, K (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM kirk.knobelspiesse@nasa.gov
RI Tsigaridis, Kostas/K-8292-2012; van Diedenhoven, Bastiaan/A-2002-2013;
Mishchenko, Michael/D-4426-2012; Knobelspiesse, Kirk/S-5902-2016;
OI Tsigaridis, Kostas/0000-0001-5328-819X; Knobelspiesse,
Kirk/0000-0001-5986-1751; van Diedenhoven, Bastiaan/0000-0001-5622-8619;
Cairns, Brian/0000-0002-1980-1022
FU NASA Postdoctoral Program at the NASA Goddard Institute for Space
Studies; NASA Headquarters under the NASA Earth and Space Science
Fellowship Program [NNX-10AN85H]; NASA; NASA ACE Formulation Study
FX Gunnar Myhre is gratefully acknowledged for providing the OsloCTM2
results. OsloCTM2 participates in the AeroCom phase 2 model
intercomparison project (http://aerocom.met.no). Kirk Knobelspiesses
participation in this research was supported by an appointment to the
NASA Postdoctoral Program at the NASA Goddard Institute for Space
Studies, administered by Oak Ridge Associated Universities through a
contract with NASA. William Martin is supported by NASA Headquarters
under the NASA Earth and Space Science Fellowship Program, Grant
NNX-10AN85H. We acknowledge funding support from the NASA Glory Mission
Project administered by Hal Maring and from the NASA ACE Formulation
Study administered by David O'C. Starr.
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PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD SEP 10
PY 2012
VL 20
IS 19
BP 21457
EP 21484
DI 10.1364/OE.20.021457
PG 28
WC Optics
SC Optics
GA 007CE
UT WOS:000308865600086
PM 23037267
ER
PT J
AU Headley, R
Hallet, B
Roe, G
Waddington, ED
Rignot, E
AF Headley, Rachel
Hallet, Bernard
Roe, Gerard
Waddington, Edwin D.
Rignot, Eric
TI Spatial distribution of glacial erosion rates in the St. Elias range,
Alaska, inferred from a realistic model of glacier dynamics
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
ID ACTIVE MOUNTAIN BELTS; ICE-THICKNESS; LANDSCAPE EVOLUTION; MALASPINA
GLACIER; SUBGLACIAL WATER; SOUTHEAST ALASKA; GLOBAL CLIMATE; OROGENIC
WEDGE; SURFACE SLOPE; NORTH PACIFIC
AB Glaciers have been principal erosional agents in many orogens throughout much of the recent geological past. A modern example is the St. Elias Mountains in southeastern Alaska; it is a highly convergent, complex orogen, which has been glaciated for much of its history. We examine the Seward-Malaspina Glacier system, which comprises two of the largest temperate glaciers in the world. We focus on the pattern of erosion within its narrow passage through the St. Elias Mountains, the Seward Throat. Measured glacier surface velocities and elevations provide constraints for a full-stress numerical flowband model that enables us to quantitatively determine the glacier thickness profile, which is not easily measured on temperate glaciers, and the basal characteristics relevant for erosion. These characteristics at the bed, namely the water pressure, normal and shear stresses, and sliding velocity, are then used to infer the spatial variation in erosion rates using several commonly invoked erosion laws. The calculations show that the geometry of the glacier basin exerts a far stronger control on the spatial variation of erosion rates than does the equilibrium line altitude, which is often assumed to be important in studies of glaciated orogens. The model provides a quantitative basis for understanding why erosion rates are highest around the Seward Throat, which is generally consistent with local and large-scale geological observations and thermochronologic evidence. Moreover, model results suggest how glacier characteristics could be used to infer zones of active or recent uplift in ice-mantled orogens.
C1 [Headley, Rachel; Hallet, Bernard; Roe, Gerard; Waddington, Edwin D.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Headley, R (reprint author), Univ Tubingen, Inst Geowissensch, Wilhelmstr 56, D-72074 Tubingen, Germany.
EM rheadley@u.washington.edu
RI Rignot, Eric/A-4560-2014
OI Rignot, Eric/0000-0002-3366-0481
FU National Science Foundation within St. Elias Erosion and Tectonics
Project (STEEP) [0409884, EAR-0735402]
FX This material is based upon work supported by the National Science
Foundation under grant 0409884 and EAR-0735402 within the St. Elias
Erosion and Tectonics Project (STEEP). We gladly thank Howard Conway for
providing data on the ice thickness, Evan Burgess for discussing the
temporal variation of the velocity through the Seward Throat, Adam
Campbell and Bruce Finlayson for invaluable help with the COMSOL
Multiphysics (R) modeling environment, and Julie Elliot for discussions
about the St. Elias geodetics. Finally, we thank Frederic Herman, Dylan
Ward, Nicholas Golledge, and the JGR editor, Bryn Hubbard, for very
helpful and in-depth reviews.
NR 89
TC 5
Z9 5
U1 1
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD SEP 8
PY 2012
VL 117
AR F03027
DI 10.1029/2011JF002291
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA 003FR
UT WOS:000308594100001
ER
PT J
AU Dalton, JB
Pitman, KM
AF Dalton, J. B., III
Pitman, K. M.
TI Low temperature optical constants of some hydrated sulfates relevant to
planetary surfaces
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID INFRARED MAPPING SPECTROMETER; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY;
MU-M; OMEGA/MARS EXPRESS; CRYSTALLINE H2O-ICE; ICE MIXTURES; MARS;
SPECTRA; MINERALS; MODEL
AB We derive optical constants (n(lambda) and k(lambda)) from laboratory reflectance spectra acquired at visible to near-infrared wavelengths for epsomite (MgSO4 center dot 7H(2)O), bloedite (Na2Mg(SO4)(2)center dot 4H(2)O), and hexahydrite (MgSO4 center dot 6H(2)O) at both room temperature and 120 K. These hydrated sulfates are candidate surface compounds for outer solar system icy satellites such as Europa, Ganymede, and Callisto, as well as Mars. Our results permit quantitative abundance modeling of Galileo, Cassini-Huygens, New Horizons, Mars Reconnaissance Orbiter, Mars Express, and future mission spacecraft observations leading to better interpretation of these objects' surface and interior geological processes and histories.
C1 [Dalton, J. B., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pitman, K. M.] Planetary Sci Inst, Tucson, AZ USA.
RP Dalton, JB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM james.b.dalton@jpl.nasa.gov
FU NASA's Outer Planets Research, Mars Fundamental Research, and Planetary
Geology and Geophysics Programs; NASA
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract to the National Aeronautics and
Space Administration. We gratefully acknowledge the support of NASA's
Outer Planets Research, Mars Fundamental Research, and Planetary Geology
and Geophysics Programs. We thank E. A. Cloutis and an anonymous
reviewer for providing helpful comments that enhanced the presentation
of this work and R. N. Clark, J. Crowley, G. B. Hansen, C. S. Jamieson,
M. D. Lane, A. R. Morgan, E. Z. Noe Dobrea, K. Snook, Y. Shkuratov, and
M. J. Wolff for providing samples, spectra, and helpful comments.
Software for continuum-removed absorption band depth analysis was
developed by G. Ruane with support from the NASA Planetary Geology and
Geophysics Undergraduate Research Program.
NR 133
TC 10
Z9 10
U1 1
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP 6
PY 2012
VL 117
AR E09001
DI 10.1029/2011JE004036
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 030AM
UT WOS:000310540000001
ER
PT J
AU Denton, RE
Sonnerup, BUO
Swisdak, M
Birn, J
Drake, JF
Hesse, M
AF Denton, R. E.
Sonnerup, B. U. Oe.
Swisdak, M.
Birn, J.
Drake, J. F.
Hesse, M.
TI Test of Shi et al. method to infer the magnetic reconnection geometry
from spacecraft data: MHD simulation with guide field and antiparallel
kinetic simulation
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CLUSTER; MOTION
AB When analyzing data from an array of spacecraft (such as Cluster or MMS) crossing a site of magnetic reconnection, it is desirable to be able to accurately determine the orientation of the reconnection site. If the reconnection is quasi-two dimensional, there are three key directions, the direction of maximum inhomogeneity (the direction across the reconnection site), the direction of the reconnecting component of the magnetic field, and the direction of rough invariance (the "out of plane" direction). Using simulated spacecraft observations of magnetic reconnection in the geomagnetic tail, we extend our previous tests of the direction-finding method developed by Shi et al. (2005) and the method to determine the structure velocity relative to the spacecraft V-str. These methods require data from four proximate spacecraft. We add artificial noise and calibration errors to the simulation fields, and then use the perturbed gradient of the magnetic field B and perturbed time derivative dB/dt, as described by Denton et al. (2010). Three new simulations are examined: a weakly three-dimensional, i.e., quasi-two-dimensional, MHD simulation without a guide field, a quasi-two-dimensional MHD simulation with a guide field, and a two-dimensional full dynamics kinetic simulation with inherent noise so that the apparent minimum gradient was not exactly zero, even without added artificial errors. We also examined variations of the spacecraft trajectory for the kinetic simulation. The accuracy of the directions found varied depending on the simulation and spacecraft trajectory, but all the directions could be found within about 10 degrees for all cases. Various aspects of the method were examined, including how to choose averaging intervals and the best intervals for determining the directions and velocity. For the kinetic simulation, we also investigated in detail how the errors in the inferred gradient directions from the unmodified Shi et al. method (using the unperturbed gradient) depended on the amplitude of the calibration errors. For an accuracy of 3 degrees for the maximum gradient direction, the calibration errors could be as large as 3% of reconnection magnetic field, while for the same accuracy for the minimum gradient direction, the calibration errors could only be as large as 0.03% of the reconnection magnetic field. These results suggest that the maximum gradient direction can normally be determined by the unmodified Shi et al. method, while the modified method or some other method must be used to accurately determine the minimum gradient direction. The structure velocity was found with magnitude accurate to 2% and direction accurate to within 5%.
C1 [Denton, R. E.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Sonnerup, B. U. Oe.] Dartmouth Coll, Thayer Sch Engn, Hanover, NH 03755 USA.
[Swisdak, M.; Drake, J. F.] Univ Maryland, Inst Res & Elect & Appl Phys, College Pk, MD 20742 USA.
[Birn, J.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Denton, RE (reprint author), Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
EM richard.e.denton@dartmouth.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA [NNX08AV81G]; NSF [ATM-0120950]; NASA
FX RED was supported primarily by NASA grant NNX08AV81G (MMS Theory
Program), and to a lesser extent by NSF grant ATM-0120950 (Center for
Integrated Space Weather Modeling, CISM, funded by the NSF Science and
Technology Centers Programs). JB acknowledges NASA support through the
MMS and Solar-Heliophysics Theory programs.
NR 15
TC 7
Z9 7
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 6
PY 2012
VL 117
AR A09201
DI 10.1029/2012JA017877
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030AR
UT WOS:000310540500007
ER
PT J
AU Sundberg, T
Slavin, JA
Boardsen, SA
Anderson, BJ
Korth, H
Ho, GC
Schriver, D
Uritsky, VM
Zurbuchen, TH
Raines, JM
Baker, DN
Krimigis, SM
McNutt, RL
Solomon, SC
AF Sundberg, Torbjoern
Slavin, James A.
Boardsen, Scott A.
Anderson, Brian J.
Korth, Haje
Ho, George C.
Schriver, David
Uritsky, Vadim M.
Zurbuchen, Thomas H.
Raines, Jim M.
Baker, Daniel N.
Krimigis, Stamatios M.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI MESSENGER observations of dipolarization events in Mercury's magnetotail
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID BURSTY BULK FLOWS; STEADY MAGNETOSPHERIC CONVECTION; CENTRAL PLASMA
SHEET; HIGH-SPEED FLOWS; FLUX TUBES; MAGNETIC RECONNECTION;
ACCELERATION; FIELD; INSTRUMENT; PARTICLE
AB Several series of large dipolarization events are documented from magnetic field observations in Mercury's magnetotail made by the MESSENGER spacecraft. The dipolarizations are identified by a rapid (similar to 1 s) increase in the northward component of the magnetic field, followed by a slower return (similar to 10 s) to pre-onset values. The changes in field strength during an event frequently reach 40 nT or higher, equivalent to an increase in the total magnetic field magnitude by a factor of similar to 4 or more. The presence of spatially constrained dipolarizations at Mercury provides a key to understanding the magnetic substorm process in a new parameter regime: the dipolarization timescale, which is shorter than at Earth, is suspected to lead to efficient non-adiabatic heating of the plasma sheet proton population, and the high recurrence rate of the structures is similar to that frequently observed for flux ropes and traveling compression regions in Mercury's magnetotail. The relatively short lifetime of the events is attributed to the lack of steady field-aligned current systems at Mercury.
C1 [Sundberg, Torbjoern; Boardsen, Scott A.; Uritsky, Vadim M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Slavin, James A.; Zurbuchen, Thomas H.; Raines, Jim M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Anderson, Brian J.; Korth, Haje; Ho, George C.; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Schriver, David] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Uritsky, Vadim M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Krimigis, Stamatios M.] Acad Athens, Athens, Greece.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Sundberg, T (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM torbjorn.sundberg@nasa.gov
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010; Ho, George/G-3650-2015
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166;
Ho, George/0000-0003-1093-2066
FU NASA Discovery Program [NAS5-97271, NASW-00002]; NASA Postdoctoral
Program at the Goddard Space Flight Center
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to The Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington.
This research was also supported by the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA.
NR 60
TC 37
Z9 37
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 6
PY 2012
VL 117
AR A00M03
DI 10.1029/2012JA017756
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030AR
UT WOS:000310540500005
ER
PT J
AU Giles, DM
Holben, BN
Eck, TF
Sinyuk, A
Smirnov, A
Slutsker, I
Dickerson, RR
Thompson, AM
Schafer, JS
AF Giles, D. M.
Holben, B. N.
Eck, T. F.
Sinyuk, A.
Smirnov, A.
Slutsker, I.
Dickerson, R. R.
Thompson, A. M.
Schafer, J. S.
TI An analysis of AERONET aerosol absorption properties and classifications
representative of aerosol source regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; LIGHT-ABSORPTION; BLACK
CARBON; WAVELENGTH DEPENDENCE; ANGSTROM EXPONENT; RADIATIVE IMPACT; IR
WAVELENGTHS; BROWN CARBON; SAHARAN DUST
AB Partitioning of mineral dust, pollution, smoke, and mixtures using remote sensing techniques can help improve accuracy of satellite retrievals and assessments of the aerosol radiative impact on climate. Spectral aerosol optical depth (T) and single scattering albedo (omega(o)) from Aerosol Robotic Network (AERONET) measurements are used to form absorption (i.e., omega(o) and absorption angstrom ngstrom exponent (alpha(abs))) and size (i.e., extinction angstrom ngstrom exponent (alpha(ext)) and fine mode fraction of T) relationships to infer dominant aerosol types. Using the long-term AERONET data set (1999-2010), 19 sites are grouped by aerosol type based on known source regions to (1) determine the average omega(o) and alpha(abs) at each site (expanding upon previous work), (2) perform a sensitivity study on alpha(abs) by varying the spectral omega(o), and (3) test the ability of each absorption and size relationship to distinguish aerosol types. The spectral omega(o) averages indicate slightly more aerosol absorption (i.e., a 0.0 < delta omega(o) <= 0.02 decrease) than in previous work, and optical mixtures of pollution and smoke with dust show stronger absorption than dust alone. Frequency distributions of alpha(abs) show significant overlap among aerosol type categories, and at least 10% of the alpha(abs) retrievals in each category are below 1.0. Perturbing the spectral omega(o) by +/- 0.03 induces significant alpha(abs) changes from the unperturbed value by at least similar to +/- 0.6 for Dust, similar to +/- 0.2 for Mixed, and similar to +/- 0.1 for Urban/Industrial and Biomass Burning. The omega(o440nm) and alpha(ext440-870nm) relationship shows the best separation among aerosol type clusters, providing a simple technique for determining aerosol type from surface-and future space-based instrumentation.
C1 [Giles, D. M.; Sinyuk, A.; Smirnov, A.; Slutsker, I.; Schafer, J. S.] Sigma Space Corp, Lanham, MD 20706 USA.
[Giles, D. M.; Holben, B. N.; Eck, T. F.; Sinyuk, A.; Smirnov, A.; Slutsker, I.; Schafer, J. S.] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Giles, D. M.; Dickerson, R. R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Eck, T. F.] Univ Space Res Assoc, Columbia, MD USA.
[Thompson, A. M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
RP Giles, DM (reprint author), Sigma Space Corp, Lanham, MD 20706 USA.
EM david.m.giles@nasa.gov
RI Thompson, Anne /C-3649-2014; Smirnov, Alexander/C-2121-2009;
OI Thompson, Anne /0000-0002-7829-0920; Smirnov,
Alexander/0000-0002-8208-1304; Dickerson, Russell/0000-0003-0206-3083
FU NASA EOS project office; Radiation Sciences Program, NASA Headquarters
FX The NASA AERONET project is supported by the NASA EOS project office and
the Radiation Sciences Program, NASA Headquarters. We would like to
thank the following principal investigators and their staff for
maintaining the following sites: Didier Tanre (Banizoumbou, Capo Verde,
Dakar, and Ouagadougou), Naif Al-Abbadi (Solar Village), Rachel Pinker
(Ilorin), Sachi Tripathi and Ramesh Singh (Kanpur), Arnon Karnieli (SEDE
BOKER), Pucai Wang (XiangHe), Giuseppe Zibordi (Ispra), Amando L.
Contreras (Mexico City), Alexander Aculinin (Moldova), Itaru Sano
(Shirahama), Paulo Artaxo (Abracos Hill and Alta Floresta), John Vande
Castle (Bonanza Creek), and Ross Mitchell (Lake Argyle). Finally, the
authors thank the AERONET team for calibrating and maintaining
instrumentation and processing these data.
NR 71
TC 84
Z9 86
U1 2
U2 65
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 6
PY 2012
VL 117
AR D17203
DI 10.1029/2012JD018127
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 029ZR
UT WOS:000310537900008
ER
PT J
AU Wade, AR
McKenzie, K
Chen, YB
Shaddock, DA
Chow, JH
McClelland, DE
AF Wade, Andrew R.
McKenzie, Kirk
Chen, Yanbei
Shaddock, Daniel A.
Chow, Jong H.
McClelland, David E.
TI Polarization speed meter for gravitational-wave detection
SO PHYSICAL REVIEW D
LA English
DT Article
ID 2-PHOTON QUANTUM OPTICS; FORMALISM
AB We propose a modified configuration of an advanced gravitational-wave detector that is a speed-meter-type interferometer with improved sensitivity with respect to quantum noise. With the addition of polarization-controlling components to the output of an arm cavity Michelson interferometer, an orthogonal polarization state of the interferometer can be used to store signal, returning it later with opposite phase to cancel position information below the storage bandwidth of the opposite mode. This modification provides an alternative to an external kilometer-scale Fabry-Perot cavity, as presented in earlier work of Purdue and Chen [Phys. Rev. D 66, 122004 (2002)]. The new configuration requires significantly less physical infrastructure to achieve speed meter operation. The quantity of length and alignment degrees of freedom is also reduced. We present theoretical calculations to show that such a speed meter detector is capable of beating the strain sensitivity imposed by the standard quantum limit over a broad range of frequencies for Advanced Laser Interferometer Gravitational-wave Observatory-like parameters. The benefits and possible difficulties of implementing such a scheme are outlined. We also present results for tuning of the speed meter by adjusting the degree of polarization coupling, a novel possibility that does not exist in previously proposed designs, showing that there is a smooth transition from speed meter operation to that of a signal-recycling Michelson behavior.
C1 [Wade, Andrew R.; Shaddock, Daniel A.; Chow, Jong H.; McClelland, David E.] Australian Natl Univ, Dept Quantum Sci, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
[McKenzie, Kirk] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chen, Yanbei] CALTECH, Pasadena, CA 91125 USA.
RP Wade, AR (reprint author), Australian Natl Univ, Dept Quantum Sci, Ctr Gravitat Phys, GPO Box 4, Canberra, ACT 0200, Australia.
RI Chen, Yanbei/A-2604-2013; McClelland, David/E-6765-2010; Shaddock,
Daniel/A-7534-2011; Chow, Jong/A-3183-2008
OI McClelland, David/0000-0001-6210-5842; Shaddock,
Daniel/0000-0002-6885-3494; Chow, Jong/0000-0002-2414-5402
FU Australian Research Council; National Science Foundation under NSF
[PHY-1068881, PHY-0956189]
FX We thank Stanley E. Whitcomb and Rana Adhikari for advice and the LIGO
Scientific Collaboration reviewers for improvements to this paper. We
also gratefully acknowledge funding support from the Australian Research
Council and the National Science Foundation under NSF Grant No.
PHY-1068881 and CAREER Grant No. PHY-0956189.
NR 18
TC 8
Z9 8
U1 1
U2 5
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 SEP 5
PY 2012
VL 86
IS 6
AR 062001
DI 10.1103/PhysRevD.86.062001
PG 8
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 999WL
UT WOS:000308345900005
ER
PT J
AU Wennberg, PO
Mui, W
Wunch, D
Kort, EA
Blake, DR
Atlas, EL
Santoni, GW
Wofsy, SC
Diskin, GS
Jeong, S
Fischer, ML
AF Wennberg, Paul O.
Mui, Wilton
Wunch, Debra
Kort, Eric A.
Blake, Donald R.
Atlas, Elliot L.
Santoni, Gregory W.
Wofsy, Steven C.
Diskin, Glenn S.
Jeong, Seongeun
Fischer, Marc L.
TI On the Sources of Methane to the Los Angeles Atmosphere
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID EMISSIONS; ETHANE; AIR
AB We use historical and new atmospheric trace gas observations to refine the estimated source of methane (CH4) emitted into California's South Coast Air Basin (the larger Los Angeles metropolitan region). Referenced to the California Air Resources Board (CARB) CO emissions inventory, total CH4 emissions are 0.44 +/- 0.15 Tg each year. To investigate the possible contribution of fossil fuel emissions, we use ambient air observations of methane (CH4), ethane (C2H6), and carbon monoxide (CO), together with measured C2H6 to CH4 enhancement ratios in the Los Angeles natural gas supply. The observed atmospheric C2H6 to CH4 ratio during the ARCTAS (2008) and CalNex (2010) aircraft campaigns is similar to the ratio of these gases in the natural gas supplied to the basin during both these campaigns. Thus, at the upper limit (assuming that the only major source of atmospheric C2H6 is fugitive emissions from the natural gas infrastructure) these data are consistent with the attribution of most (0.39 +/- 0.15 Tg yr(-1)) of the excess CH4 in the basin to uncombusted losses from the natural gas system (approximately 2.5-6% of natural gas delivered to basin customers). However, there are other sources of C2H6 in the region. In particular, emissions of C2H6 (and CH4) from natural gas seeps as well as those associated with petroleum production, both of which are poorly known, will reduce the inferred contribution of the natural gas infrastructure to the total CH4 emissions, potentially significantly. This study highlights both the value and challenges associated with the use of ethane as a tracer for fugitive emissions from the natural gas production and distribution system.
C1 [Wennberg, Paul O.; Mui, Wilton] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[Wennberg, Paul O.; Wunch, Debra] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Kort, Eric A.] CALTECH, Keck Inst Space Studies, Pasadena, CA 91125 USA.
[Blake, Donald R.] Univ Calif Irvine, Sch Phys Sci, Irvine, CA 92697 USA.
[Atlas, Elliot L.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Santoni, Gregory W.; Wofsy, Steven C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02318 USA.
[Santoni, Gregory W.; Wofsy, Steven C.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02318 USA.
[Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Jeong, Seongeun; Fischer, Marc L.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Environm Energy Technol Div, Berkeley, CA 94720 USA.
RP Wennberg, PO (reprint author), CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
EM wennberg@caltech.edu
RI Kort, Eric/F-9942-2012; Wennberg, Paul/A-5460-2012; Atlas,
Elliot/J-8171-2015
OI Kort, Eric/0000-0003-4940-7541;
FU NASA; NOAA; California Air Resources Board; California Institute of
Technology; NSF Graduate Research Fellowship; W.M. Keck Institute for
Space Studies; NSF; EPA; California Energy Commission's Public Interest
Environmental Research (CEC-PIER) program; US Dept. of Energy through
the LBNL Laboratory Directed Research and Development
[DE-ACO2-05CH11231]
FX Data used in this analysis were obtained with support of NASA, NOAA, and
the California Air Resources Board. We thank Stephanie A. Vay for her
efforts to obtain the CO2 data during ARCTAS. We thank the
Southern California Gas Company for their interest and support in this
study. The analysis was supported by the California Institute of
Technology. Support for the analysis of the remote sensing data was
provided by NASA's Terrestrial Ecology Program. W.M. acknowledges
support from a NSF Graduate Research Fellowship. This work was funded in
part by the W.M. Keck Institute for Space Studies. G.S. acknowledges
support from NSF and EPA STAR graduate fellowships. We thank Joseph
Fischer, Larry Hunsaker, Webster Tassat, Marc Vayssieres, and Ying-Kang
Hsu for sharing advice and data. This work was supported by the
California Energy Commission's Public Interest Environmental Research
(CEC-PIER) program, the California Air Resources Board, and the US Dept.
of Energy through the LBNL Laboratory Directed Research and Development,
under contract No. DE-ACO2-05CH11231.
NR 37
TC 51
Z9 52
U1 4
U2 68
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD SEP 4
PY 2012
VL 46
IS 17
BP 9282
EP 9289
DI 10.1021/es301138y
PG 8
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 998SM
UT WOS:000308260700010
PM 22853880
ER
PT J
AU Henze, DK
Shindell, DT
Akhtar, F
Spurr, RJD
Pinder, RW
Loughlin, D
Kopacz, M
Singh, K
Shim, C
AF Henze, Daven K.
Shindell, Drew T.
Akhtar, Farhan
Spurr, Robert J. D.
Pinder, Robert W.
Loughlin, Dan
Kopacz, Monika
Singh, Kumaresh
Shim, Changsub
TI Spatially Refined Aerosol Direct Radiative Forcing Efficiencies
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID NEXT-GENERATION; AIR-QUALITY; CLIMATE; MODELS; SATELLITE; EMISSIONS;
TRANSPORT; STABILIZATION; CONSTRAINTS; DEPOSITION
AB Global aerosol direct radiative forcing (DRF) is an important metric for assessing potential climate impacts of future emissions changes. However, the radiative consequences of emissions perturbations are not readily quantified nor well understood at the level of detail necessary to assess realistic policy options. To address this challenge, here we show how adjoint model sensitivities can be used to provide highly spatially resolved estimates of the DRF from emissions of black carbon (BC), primary organic carbon (OC), sulfur dioxide (SO2), and ammonia (NH3), using the example of emissions from each sector and country following multiple Representative Concentration Pathway (RCPs). The radiative forcing efficiencies of many individual emissions are found to differ considerably from regional or sectoral averages for NH3, SO2 from the power sector, and BC from domestic, industrial, transportation and biomass burning sources. Consequently, the amount of emissions controls required to attain a specific DRF varies at intracontinental scales by up to a factor of 4. These results thus demonstrate both a need and means for incorporating spatially refined aerosol DRF into analysis of future emissions scenario and design of air quality and climate change mitigation policies.
C1 [Henze, Daven K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
[Shindell, Drew T.] Columbia Univ, New York, NY 10025 USA.
[Shindell, Drew T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Akhtar, Farhan; Pinder, Robert W.; Loughlin, Dan] US EPA, Off Res & Dev, Res Triangle Pk, NC 27711 USA.
[Spurr, Robert J. D.] RT Solut Inc, Cambridge, MA 02138 USA.
[Kopacz, Monika] NOAA, Climate Program Off, Silver Spring, MD USA.
[Singh, Kumaresh] Virginia Polytech Inst & State Univ, Dept Comp Sci, Blacksburg, VA 24061 USA.
[Shim, Changsub] Korea Environm Inst, Seoul, South Korea.
RP Henze, DK (reprint author), Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
EM daven.henze@colorado.edu
RI Pinder, Robert/F-8252-2011; Chem, GEOS/C-5595-2014; Shindell,
Drew/D-4636-2012; Singh, Kumaresh/P-4857-2016
OI Pinder, Robert/0000-0001-6390-7126;
FU NASA [NNH09ZDA001N]; NASA AQAST [NNH09ZDA001N]
FX D.K.H. recognizes support from the NASA New Investigator Program
(NNH09ZDA001N), NASA AQAST (NNH09ZDA001N), and use of NASA HEC computing
facilities. While this manuscript has been reviewed by EPA and approved
for publication, it does not necessarily reflect official agency views
or policies.
NR 65
TC 16
Z9 16
U1 4
U2 37
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD SEP 4
PY 2012
VL 46
IS 17
BP 9511
EP 9518
DI 10.1021/es301993s
PG 8
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 998SM
UT WOS:000308260700036
PM 22881708
ER
PT J
AU Yu, ZH
Herndon, SC
Ziemba, LD
Timko, MT
Liscinsky, DS
Anderson, BE
Miake-Lye, RC
AF Yu, Zhenhong
Herndon, Scott C.
Ziemba, Luke D.
Timko, Michael T.
Liscinsky, David S.
Anderson, Bruce E.
Miake-Lye, Richard C.
TI Identification of Lubrication Oil in the Particulate Matter Emissions
from Engine Exhaust of In-Service Commercial Aircraft
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID AEROSOL MASS-SPECTROMETER; ATLANTA-INTERNATIONAL-AIRPORT; CRUISE
CONDITIONS; TRACE GAS; DISTRIBUTIONS; ESTERS; SIZE; PLUMES; URBAN
AB Lubrication oil was identified in the organic particulate matter (PM) emissions of engine exhaust plumes from in-service commercial aircraft at Chicago Midway Airport (MDW) and O'Hare International Airport (ORD). This is the first field study focused on aircraft lubrication oil emissions, and all of the observed plumes described in this work were due to near-idle engine operations. The identification was carried out with an Aerodyne high-resolution time-of-flight aerosol mass spectrometer (HR-ToF AMS) via a collaborative laboratory and field investigation. A characteristic mass marker of lubrication oil, I(85)/I(71), the ratio of ion fragment intensity between m/z = 85 and 71, was used to distinguish lubrication oil from jet engine combustion products. This AMS marker was based on ion fragmentation patterns measured using electron impact ionization for two brands of widely used lubrication oil in a laboratory study. The AMS measurements of exhaust plumes from commercial aircraft in this airport field study reveal that lubrication oil is commonly present in organic PM emissions that are associated with emitted soot particles, unlike the purely oil droplets observed at the lubrication system vent. The characteristic oil marker, I(85)/I(71), was applied to quantitatively determine the contribution from lubrication oil in measured aircraft plumes, which ranges from 5% to 100%.
C1 [Yu, Zhenhong; Herndon, Scott C.; Timko, Michael T.; Miake-Lye, Richard C.] Aerodyne Res Inc, Billerica, MA 01821 USA.
[Ziemba, Luke D.; Anderson, Bruce E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Liscinsky, David S.] United Technol Res Ctr, E Hartford, CT 06108 USA.
RP Yu, ZH (reprint author), Aerodyne Res Inc, Billerica, MA 01821 USA.
EM zyu@aerodyne.com
FU Airport Cooperative Research Program (ACRP) project [02-03a]; U.S.
Department of Defense; NASA (NRA) [NNC07CB57C]
FX This research was supported by the Airport Cooperative Research Program
(ACRP) project 02-03a, the U.S. Department of Defense, through the
Strategic Environmental Research and Development Program (SERDP), and
NASA (NRA #NNC07CB57C). We thank Southwest Airlines, United Airlines,
and the City of Chicago for providing us access to taxiways in the
airports and the invaluable support to conduct measurements at MDW and
ORD. We are also grateful for the assistance and logistical support
offered by John Jayne, Bill Brooks, and Tim Onasch at ART during
instrument preparation activities and laboratory studies.
NR 41
TC 7
Z9 7
U1 1
U2 20
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD SEP 4
PY 2012
VL 46
IS 17
BP 9630
EP 9637
DI 10.1021/es301692t
PG 8
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 998SM
UT WOS:000308260700052
PM 22870990
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.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA.
NR 0
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 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2012
VL 2
IS 5
BP 473
EP 473
DI 10.1109/TTHZ.2012.2212294
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AM
UT WOS:000318768100001
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, SWAT Team, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA.
NR 1
TC 2
Z9 2
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 SEP
PY 2012
VL 2
IS 5
BP 477
EP 477
DI 10.1109/TTHZ.2012.2212078
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AM
UT WOS:000318768100002
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneer: Thomas G. Phillips "The Sky Above, the Mountain
Below"
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
ID ORION MOLECULAR CLOUD; WAVE-GUIDE RECEIVER; SINGLE-ION MAGNETOSTRICTION;
TUNNEL-JUNCTION MIXERS; CARBON-MONOXIDE; MILLIMETER-WAVE; LINE SURVEY;
ATOMIC CARBON; SIS MIXERS; SUBMILLIMETER ASTRONOMY
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.
EM phs@caltech.edu
NR 85
TC 3
Z9 3
U1 0
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2012
VL 2
IS 5
BP 478
EP 484
DI 10.1109/TTHZ.2012.2211353
PG 7
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AM
UT WOS:000318768100003
ER
PT J
AU Blinzler, BJ
Goldberg, RK
Binienda, WK
AF Blinzler, Brina J.
Goldberg, Robert K.
Binienda, Wieslaw K.
TI Macroscale Independently Homogenized Subcells for Modeling Braided
Composites
SO AIAA JOURNAL
LA English
DT Article
AB An analytical method has been developed to analyze the impact response of triaxially braided carbon fiber composites, including the penetration velocity and impact damage patterns. 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. Currently, 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. To determine the stiffness and strength properties required for the constitutive model, a topdown approach for determining the strength properties is merged with a bottom-up approach for determining the stiffness properties. The top-down portion uses global strengths obtained from macro-scale coupon level testing to characterize the material strengths for each subcell. The bottom-up portion uses micro-scale fiber and matrix stiffness properties to characterize the material stiffness for each subcell. Simulations of quasi-static coupon level tests for several representative composites are conducted along with impact simulations.
C1 [Blinzler, Brina J.; Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
[Goldberg, Robert K.] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
RP Blinzler, BJ (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
FU Vehicle Systems Safety Technologies of the Aviation Safety Program; NASA
Graduate Student Researchers Program [NNXD9AL95H]
FX This work was funded by the Vehicle Systems Safety Technologies of the
Aviation Safety Program and NASA Graduate Student Researchers Program
grant number NNXD9AL95H
NR 22
TC 2
Z9 2
U1 1
U2 6
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD SEP
PY 2012
VL 50
IS 9
BP 1873
EP 1884
DI 10.2514/1.J051342
PG 12
WC Engineering, Aerospace
SC Engineering
GA 998ZH
UT WOS:000308278400017
ER
PT J
AU Roy, N
Chomiuk, L
Sokoloski, JL
Weston, J
Rupen, MP
Johnson, T
Krauss, MI
Nelson, T
Mukai, K
Mioduszewski, A
Bode, MF
Eyres, SPS
O'Brien, TJ
AF Roy, Nirupam
Chomiuk, Laura
Sokoloski, Jennifer L.
Weston, Jennifer
Rupen, Michael P.
Johnson, Traci
Krauss, Miriam I.
Nelson, Thomas
Mukai, Koji
Mioduszewski, Amy
Bode, Michael F.
Eyres, Stewart P. S.
O'Brien, Tim J.
TI Radio studies of novae: a current status report and highlights of new
results
SO BULLETIN OF THE ASTRONOMICAL SOCIETY OF INDIA
LA English
DT Article
DE novae; cataclysmic variables; radio continuum: stars; white dwarfs
ID X-RAY-EMISSION; IA SUPERNOVA PROGENITORS; CLASSICAL NOVAE; RECURRENT
NOVA; RS-OPHIUCHI; T PYXIDIS; V407 CYG; WHITE-DWARF; LARGE ARRAY; GK
PERSEI
AB Novae, which are the sudden visual brightening triggered by runaway thermonuclear burning on the surface of an accreting white dwarf, are fairly common and bright events. Despite their astronomical significance as nearby laboratories for the study of nuclear burning and accretion phenomena, many aspects of these common stellar explosions are observationally not well-constrained and remain poorly understood. Radio observations, modeling and interpretation can potentially play a crucial role in addressing some of these puzzling issues. In this review on radio studies of novae, we focus on the possibility of testing and improving the nova models with radio observations, and present a current status report on the progress in both the observational front and theoretical developments. We specifically address the issues of accurate estimation of ejecta mass, multi-phase and complex ejection phenomena, and the effect of a dense environment around novae. With highlights of new observational results, we illustrate how radio observations can shed light on some of these long-standing puzzles.
C1 [Roy, Nirupam; Chomiuk, Laura; Rupen, Michael P.; Johnson, Traci; Krauss, Miriam I.; Mioduszewski, Amy] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Sokoloski, Jennifer L.; Weston, Jennifer] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Johnson, Traci] Carleton Coll, Dept Phys & Astron, Northfield, MN 55057 USA.
[Nelson, Thomas] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Mukai, Koji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Mukai, Koji] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Mukai, Koji] Univ Maryland Baltimore Cty, Ctr Space Sci & Tech, Baltimore, MD 21250 USA.
[Bode, Michael F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Eyres, Stewart P. S.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[O'Brien, Tim J.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
RP Roy, N (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
EM nroy@nrao.edu
NR 89
TC 7
Z9 7
U1 0
U2 4
PU INDIAN INST ASTROPHYSICS
PI BANGALORE
PA G C ANUPAMA EDITOR, BANGALORE, 560 034, INDIA
SN 0304-9523
J9 B ASTRON SOC INDIA
JI Bull. Astron. Soc. India.
PD SEP
PY 2012
VL 40
IS 3
BP 293
EP 310
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 081ML
UT WOS:000314326200007
ER
PT J
AU Zeng, J
Kukreja, SL
Moulin, B
AF Zeng, Jie
Kukreja, Sunil L.
Moulin, Boris
TI Experimental Model-Based Aeroelastic Control for Flutter Suppression and
Gust-Load Alleviation
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA Atmospheric Flight Mechanics Conference / AIAA Modeling and
Simulation Technologies Conference / AIAA Guidance, Navigation, and
Control Conference
CY AUG 08-11, 2011
CL Portland, OR
SP AIAA
AB This paper introduces an experimental model-based feedback-control framework for flutter suppression and gust load alleviation. With the proposed experimental model-based feedback-control framework, the flexible dynamics can be consistently estimated via system-identification algorithms, and its undesirable effects are suppressed through a robust feedback-control law while the whole system's stability is being maintained. Therefore, the resilience of the flight control law in the presence of aeroelastic/aeroservoelastic interactions can be increased by the suppression of the aircraft's structural vibrations induced by the flutter mechanism and/or gust perturbation. The proposed experimental model-based feedback-control technique is demonstrated on the SuperSonic SemiSpan Transport wind-tunnel model for flutter suppression and gust-load alleviation.
C1 [Zeng, Jie] ZONA Technol Inc, Res & Dev Control Syst, Scottsdale, AZ 85258 USA.
[Kukreja, Sunil L.] NASA Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA.
[Moulin, Boris] ZONA Technol Inc, Scottsdale, AZ 85258 USA.
RP Zeng, J (reprint author), ZONA Technol Inc, Res & Dev Control Syst, Scottsdale, AZ 85258 USA.
EM jzeng@zonatech.com; sunil.l.kukreja@nasa.gov; bsmoulin@gmail.com
NR 12
TC 2
Z9 4
U1 1
U2 7
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP-OCT
PY 2012
VL 35
IS 5
BP 1377
EP 1390
DI 10.2514/1.56790
PG 14
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 082FY
UT WOS:000314378900001
ER
PT J
AU Holzel, MS
Morelli, EA
AF Holzel, Matthew S.
Morelli, Eugene A.
TI Real-Time Frequency Response Estimation from Flight Data
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA Atmospheric Flight Mechanics Conference / AIAA Modeling and
Simulation Technologies Conference / AIAA Guidance, Navigation, and
Control Conference
CY AUG 08-11, 2011
CL Portland, OR
SP AIAA
AB A nonparametric method for estimating frequency responses in real time based on recursive least squares in the time domain was developed and studied. The method uses sinusoidal functions at selected frequencies known to be contained in the input in conjunction with recursive least squares to rapidly estimate Fourier series coefficients for input and output time series, and thereby estimate frequency responses. Practical problems that arise when applying the discrete Fourier transform in recursive form were identified using simple examples. A general expression for accurate real-time calculation of the covariance matrix for recursive least-squares parameter estimation was developed and used to calculate valid uncertainty bounds for real-time frequency response estimates. Simulation data generated with optimized multisine inputs were used to investigate the accuracy of the proposed method for real-time frequency response estimation and to validate the calculated error bounds. The approach was also applied to flight data from a subscale jet transport aircraft. Comparisons of real-time frequency response estimates and error bounds with results from conventional postflight batch analysis showed that results from the real-time method were in statistical agreement with postflight batch estimates, with valid error bounds that properly indicated the quality of the real-time frequency response estimates.
C1 [Holzel, Matthew S.] Univ Michigan, Ann Arbor, MI 48105 USA.
[Morelli, Eugene A.] NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA.
RP Holzel, MS (reprint author), Univ Michigan, Ann Arbor, MI 48105 USA.
NR 17
TC 3
Z9 3
U1 2
U2 7
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP-OCT
PY 2012
VL 35
IS 5
BP 1406
EP 1417
DI 10.2514/1.56782
PG 12
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 082FY
UT WOS:000314378900003
ER
PT J
AU Morgan, D
Chung, SJ
Blackmore, L
Acikmese, B
Bayard, D
Hadaegh, FY
AF Morgan, Daniel
Chung, Soon-Jo
Blackmore, Lars
Acikmese, Behcet
Bayard, David
Hadaegh, Fred Y.
TI Swarm-Keeping Strategies for Spacecraft Under J2 and Atmospheric Drag
Perturbations
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA Atmospheric Flight Mechanics Conference / AIAA Modeling and
Simulation Technologies Conference / AIAA Guidance, Navigation, and
Control Conference
CY AUG 08-11, 2011
CL Portland, OR
SP AIAA
ID FORMATION-FLYING SPACECRAFT; RELATIVE MOTION; ELLIPTIC ORBIT; GUIDANCE;
EQUATIONS; DYNAMICS; ELEMENTS
AB This paper presents several new open-loop guidance methods for spacecraft swarms composed of hundreds to thousands of agents, with each spacecraft having modest capabilities. These methods have three main goals: preventing relative drift of the swarm, preventing collisions within the swarm, and minimizing the propellant used throughout the mission. The development of these methods progresses by eliminating drift using the Hill-Clohessy-Wiltshire equations, removing drift due to nonlinearity, and minimizing the J(2) drift. To verify these guidance methods, a new dynamic model for the relative motion of spacecraft is developed. These dynamics include the two main disturbances for spacecraft in low Earth orbit, J(2) and atmospheric drag. Using this dynamic model, numerical simulations are provided at each step to show the effectiveness of each method and to see where improvements can be made. The main result is a set of initial conditions for each spacecraft in the swarm, which provides the trajectories for hundreds of collision-free orbits in the presence of J(2). Finally, a multiburn strategy is developed to provide hundreds of collision-free orbits under the influence of atmospheric drag. This last method works by enforcing the initial conditions multiple times throughout the mission, thereby providing collision-free trajectories for the duration of the mission.
C1 [Morgan, Daniel; Chung, Soon-Jo] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
[Blackmore, Lars; Acikmese, Behcet; Bayard, David; Hadaegh, Fred Y.] CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Pasadena, CA 91109 USA.
RP Morgan, D (reprint author), Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
EM morgan29@illinois.edu; sjchung@illinois.edu; larsblackmore@gmail.com;
behcet.acikmese@jpl.nasa.gov; david.bayard@jpl.nasa.gov;
fred.y.hadaegh@jpl.nasa.gov
OI Chung, Soon-Jo/0000-0002-6657-3907
NR 28
TC 14
Z9 15
U1 2
U2 17
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP-OCT
PY 2012
VL 35
IS 5
BP 1492
EP 1506
DI 10.2514/1.55705
PG 15
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 082FY
UT WOS:000314378900011
ER
PT J
AU Scarritt, SK
Marchand, BG
Brown, AJ
Tracy, WH
Weeks, MW
AF Scarritt, S. K.
Marchand, B. G.
Brown, A. J.
Tracy, W. H.
Weeks, M. W.
TI Finite-Burn Linear Targeting Algorithm for Autonomous Path Planning and
Guidance
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY AUG 10-13, 2009
CL Chicago, IL
SP Amer Inst Aeronaut & Astronaut (AIAA)
ID TRAJECTORY DESIGN; SYSTEM; OPTIMIZATION
AB In path planning and guidance applications, linear targeting through differential corrections is a classical approach for identifying feasible solutions that meet specified mission and trajectory constraints. However, to date, these methods relied on the assumption that the associated correction maneuvers were impulsive in nature. This impulsive assumption is generally reasonable when the duration of the engine burn is small. However, this approximation breaks down when lower thrust engines are employed as the duration of the burn becomes more significant. In these cases, an impulsive linear targeting algorithm is inadequate. Often times, low-thrust problems of this type are solved from the perspective of optimal trajectory design and depend on numerical methods like nonlinear programming. These methods, however, are generally considered prohibitive for autonomous flight applications, where computational resources are limited and optimality is not always as important as feasibility. The present study focuses on the theoretical development and numerical validation of a linear targeting algorithm capable of accommodating finite burn maneuvers. Examples are presented to contrast the performance of this new targeting process against more classical impulsive targeting methods. The examples presented focus largely on precision entry applications, but the finite burn targeting process itself is applicable across a broad set of scenarios and fields.
C1 [Scarritt, S. K.; Marchand, B. G.] Univ Texas Austin, Dept Aerosp Engn, Austin, TX 78712 USA.
[Brown, A. J.] NASA, Lyndon B Johnson Space Ctr, Rendezvous Guidance & Procedures DM34, Houston, TX 77058 USA.
[Tracy, W. H.] NASA, Lyndon B Johnson Space Ctr, Orbit Flight Dynam DM32, Houston, TX 77058 USA.
[Weeks, M. W.] NASA, Lyndon B Johnson Space Ctr, Aerosci & Flight Mech Div EG 6, Houston, TX 77058 USA.
RP Marchand, BG (reprint author), Univ Texas Austin, Dept Aerosp Engn, 210 E 24th St, Austin, TX 78712 USA.
EM marchand@mail.utexas.edu
NR 23
TC 1
Z9 1
U1 0
U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP-OCT
PY 2012
VL 35
IS 5
BP 1605
EP 1615
DI 10.2514/1.54249
PG 11
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 082FY
UT WOS:000314378900020
ER
PT J
AU Lee, DW
Bass, EJ
Patek, SD
Alexandrov, N
Kincaid, RK
AF Lee, Douglas W.
Bass, Ellen J.
Patek, Stephen D.
Alexandrov, Natalia
Kincaid, Rex K.
TI Minimax Network Flow Model for Assessing Impacts of Airport Capacity
Perturbations
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
AB Policy decisions that target effective utilization of the national airspace often relate to the capacities of individual airports in the system, and decisions to increase or reduce capacity (e.g., via slot restrictions) must be supported quantitatively. It is of particular interest to assess global impacts of capacity adjustments, because addressing congestion issues at one airport may have a "ripple effect" on the utilization of capacity elsewhere in the network. In this paper, an analytical model was developed that addresses system-wide implications of capacity decisions at the level of interactions between Operational Evolution Partnership 35 airports. Two main elements comprise the model: 1) a network flow model that describes both the capacities of Operational Evolution Partnership 35 airports and the demand for aircraft serving origin-destination traffic across the network and 2) a novel mathematical program referred to as the minimax node utilization problem that, when solved, minimizes the worst-case capacity utilization across all of the airports in the network. Both elements combine to allow quick assessment of both local and global effects of airport capacity adjustments. The analytical model is evaluated via case studies, including two capacity reduction scenarios and one capacity expansion scenario, focusing on the model's ability to describe how capacity influences airport utilization throughout a network representing actual origin-destination demands in the airspace. The results from these scenarios indicate that the model provides a simple and effective technique for describing impacts of airport capacity perturbations, providing valuable high-level insight into airport utilization patterns.
C1 [Lee, Douglas W.; Bass, Ellen J.; Patek, Stephen D.] Univ Virginia, Syst & Informat Engn Dept, Charlottesville, VA 22903 USA.
[Alexandrov, Natalia] NASA, Langley Res Ctr, Syst Anal & Concepts Directorate, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA.
[Kincaid, Rex K.] Coll William & Mary, Dept Math, Williamsburg, VA 23187 USA.
RP Lee, DW (reprint author), Univ Virginia, Syst & Informat Engn Dept, Charlottesville, VA 22903 USA.
EM dwl5f@virginia.edu; ejb4n@virginia.edu; patek@virginia.edu;
n.alexandrov@nasa.gov; rrkinc@wm.edu
FU NASA [NCC1002043, NNX08AH39A]
FX The research was funded in part by NASA Cooperative Agreement NCC1002043
and NASA grant NNX08AH39A. The content is solely the responsibility of
the authors and does not necessarily represent the official views of
NASA. The authors thank the two anonymous reviewers for their many
helpful comments, which significantly improved this paper.
NR 21
TC 0
Z9 0
U1 1
U2 5
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP-OCT
PY 2012
VL 35
IS 5
BP 1616
EP 1624
DI 10.2514/1.53975
PG 9
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 082FY
UT WOS:000314378900021
ER
PT J
AU Casey, K
Kaab, A
AF Casey, Kimberly
Kaab, Andreas
TI Estimation of Supraglacial Dust and Debris Geochemical Composition via
Satellite Reflectance and Emissivity
SO REMOTE SENSING
LA English
DT Article
DE glaciology; remote sensing; supraglacial dust; tephra; reflectance;
ASTER; MODIS; Hyperion
ID NEW-ZEALAND; GLACIER INVENTORY; HYPERSPECTRAL DATA; RUAPEHU-VOLCANO;
CRATER LAKE; IN-SITU; ICELAND; ICE; SNOW; ALBEDO
AB We demonstrate spectral estimation of supraglacial dust, debris, ash and tephra geochemical composition from glaciers and ice fields in Iceland, Nepal, New Zealand and Switzerland. Surface glacier material was collected and analyzed via X-ray fluorescence spectroscopy (XRF) and X-ray diffraction (XRD) for geochemical composition and mineralogy. In situ data was used as ground truth for comparison with satellite derived geochemical results. Supraglacial debris spectral response patterns and emissivity-derived silica weight percent are presented. Qualitative spectral response patterns agreed well with XRF elemental abundances. Quantitative emissivity estimates of supraglacial SiO2 in continental areas were 67% (Switzerland) and 68% (Nepal), while volcanic supraglacial SiO2 averages were 58% (Iceland) and 56% (New Zealand), yielding general agreement. Ablation season supraglacial temperature variation due to differing dust and debris type and coverage was also investigated, with surface debris temperatures ranging from 5.9 to 26.6 degrees C in the study regions. Applications of the supraglacial geochemical reflective and emissive characterization methods include glacier areal extent mapping, debris source identification, glacier kinematics and glacier energy balance considerations.
C1 [Casey, Kimberly] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Kaab, Andreas] Univ Oslo, Dept Geosci, N-0316 Oslo, Norway.
RP Casey, K (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA.
EM kimberly.a.casey@nasa.gov; andreas.kaab@geo.uio.no
RI Casey, Kimberly/A-4478-2013
OI Casey, Kimberly/0000-0002-6115-7525
FU University of Oslo, Department of Geosciences; ESA GlobGlacier project
[21088/07/I-EC]; NASA Postdoctoral Program
FX This work was funded by the University of Oslo, Department of
Geosciences; the ESA GlobGlacier project (21088/07/I-EC) and the NASA
Postdoctoral Program administered by Oak Ridge Associated Universities.
The authors thank two anonymous reviewers and the editor for
constructive feedback. We thank M. Zemp of the World Glacier Monitoring
Service for logistic support toward Swiss Alps field work. We are
grateful to glaciologists A. Barrueto and E. Rinne for one day each
field support at Zmutt glacier. The authors thank R. Xie and B. L. Berg
of the University of Oslo for assistance with XRD and XRF analysis.
NR 72
TC 2
Z9 2
U1 8
U2 32
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2012
VL 4
IS 9
BP 2554
EP 2575
DI 10.3390/rs4092554
PG 22
WC Remote Sensing
SC Remote Sensing
GA 075UX
UT WOS:000313913500004
ER
PT J
AU Mouginot, J
Scheuchl, B
Rignot, E
AF Mouginot, Jeremie
Scheuchl, Bernd
Rignot, Eric
TI Mapping of Ice Motion in Antarctica Using Synthetic-Aperture Radar Data
SO REMOTE SENSING
LA English
DT Article
DE Antarctica; InSAR; ice motion
ID DIGITAL ELEVATION MODEL; LASER DATA; SHEET; FLOW; INTERFEROMETRY
AB Ice velocity is a fundamental parameter in studying the dynamics of ice sheets. Until recently, no complete mapping of Antarctic ice motion had been available due to calibration uncertainties and lack of basic data. Here, we present a method for calibrating and mosaicking an ensemble of InSAR satellite measurements of ice motion from six sensors: the Japanese ALOS PALSAR, the European Envisat ASAR, ERS-1 and ERS-2, and the Canadian RADARSAT-1 and RADARSAT-2. Ice motion calibration is made difficult by the sparsity of in-situ reference points and the shear size of the study area. A sensor-dependent data stacking scheme is applied to reduce measurement uncertainties. The resulting ice velocity mosaic has errors in magnitude ranging from 1 m/yr in the interior regions to 17 m/yr in coastal sectors and errors in flow direction ranging from less than 0.5 degrees in areas of fast flow to unconstrained direction in sectors of slow motion. It is important to understand how these mosaics are calibrated to understand the inner characteristics of the velocity products as well as to plan future InSAR acquisitions in the Antarctic. As an example, we show that in broad sectors devoid of ice-motion control, it is critical to operate ice motion mapping on a large scale to avoid pitfalls of calibration uncertainties that would make it difficult to obtain quality products and especially construct reliable time series of ice motion needed to detect temporal changes.
C1 [Mouginot, Jeremie; Scheuchl, Bernd; Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Rignot, Eric] Caltechs Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mouginot, J (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM jmougino@uci.edu; bscheuch@uci.edu; eric.j.rignot@jpl.nasa.gov
RI Rignot, Eric/A-4560-2014; Mouginot, Jeremie/G-7045-2015;
OI Rignot, Eric/0000-0002-3366-0481; Mouginot, Jeremie/0000-0001-9155-5455
NR 21
TC 26
Z9 27
U1 1
U2 25
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2012
VL 4
IS 9
BP 2753
EP 2767
DI 10.3390/rs4092753
PG 15
WC Remote Sensing
SC Remote Sensing
GA 075UX
UT WOS:000313913500012
ER
PT J
AU Hecht, BC
Thrower, FP
Hale, MC
Miller, MR
Nichols, KM
AF Hecht, Benjamin C.
Thrower, Frank P.
Hale, Matthew C.
Miller, Michael R.
Nichols, Krista M.
TI Genetic Architecture of Migration-Related Traits in Rainbow and
Steelhead Trout, Oncorhynchus mykiss
SO G3-GENES GENOMES GENETICS
LA English
DT Article
DE linkage mapping; migration; Oncorhynchus mykiss; QTL; RAD-tag
sequencing; smoltification
ID ANIMAL MIGRATION; SMOLT TRANSFORMATION; BODY MORPHOLOGY; WILD
POPULATION; CHINOOK SALMON; WING LENGTH; RAD MARKERS; COHO SALMON;
SEA-WATER; SMOLTIFICATION
AB Although migration plays a critical role in the evolution and diversification of species, relatively little is known of the genetic architecture underlying this life history in any species. Rainbow and steelhead trout (Oncorhynchus mykiss) naturally segregate for both resident and migratory life-history types, respectively, as do other members of the salmonid family of fishes. Using an experimental cross derived from wild resident rainbow and wild migratory steelhead trout from Southeast Alaska and high throughput restriction-site associated DNA (RAD) tag sequencing, we perform a quantitative trait locus (QTL) analysis to identify the number, position, and relative contribution of genetic effects on a suite of 27 physiological and morphological traits associated with the migratory life history in this species. In total, 37 QTL are localized to 19 unique QTL positions, explaining 4-13.63% of the variation for 19 of the 27 migration-related traits measured. Two chromosomal positions, one on chromosome Omy12 and the other on Omy14 each harbor 7 QTL for migration-related traits, suggesting that these regions could harbor master genetic controls for the migratory life-history tactic in this species. Another QTL region on Omy5 has been implicated in several studies of adaptive life histories within this species and could represent another important locus underlying the migratory life history. We also evaluate whether loci identified in this out-crossed QTL study colocalize to genomic positions previously identified for associations with migration-related traits in a doubled haploid mapping family.
C1 [Hecht, Benjamin C.; Hale, Matthew C.; Nichols, Krista M.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA.
[Nichols, Krista M.] Purdue Univ, Dept Forestry & Nat Resources, W Lafayette, IN 47907 USA.
[Thrower, Frank P.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Juneau, AK 99801 USA.
[Miller, Michael R.] Univ Oregon, Inst Mol Biol, Eugene, OR 97403 USA.
RP Nichols, KM (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA.
EM krista.nichols@noaa.gov
FU Ecological Genetics Area of Excellence in the Department of Forestry and
Natural Resources, Purdue University; [NSF-DEB-0845265]
FX The authors would like to thank Adrian Celewycz, Jeff Hard, Michael
Zanis, Jim Meyers, Melissa Baird, Orlay Johnson, Jason Miller, Pat
Malecha, and Jen Malecha, who assisted with the rearing, husbandry,
and/or data collection of rainbow and steelhead trout at the Little Port
Walter Research Station, Baranof Island, Alaska. We also acknowledge the
assistance of Steve Sassman and Linda Lee in the collection of
spectrophotometric data; Julie Scardina, Graham Wolf, Katlin Walls, and
Madeline Valle for assistance in the collection of genotype data; and
Garrett McKinney and Doug Yatcilla, who assisted with bioinformatics and
computation. We also thank two anonymous reviewers for their
tremendously insightful comments, which greatly improved this
manuscript. This work was funded in part by a NSF-DEB-0845265 Career
Award to KMN, and by funding through the Ecological Genetics Area of
Excellence in the Department of Forestry and Natural Resources, Purdue
University. The authors have no conflicts of interest to declare.
NR 76
TC 47
Z9 47
U1 5
U2 82
PU GENETICS SOC AM
PI BETHESDA
PA 9650 ROCKVILLE AVE, BETHESDA, MD 20814 USA
SN 2160-1836
J9 G3-GENES GENOM GENET
JI G3-Genes Genomes Genet.
PD SEP 1
PY 2012
VL 2
IS 9
BP 1113
EP 1127
DI 10.1534/g3.112.003137
PG 15
WC Genetics & Heredity
SC Genetics & Heredity
GA 055ZH
UT WOS:000312456100015
PM 22973549
ER
PT J
AU Pike, L
Wegmann, N
Niller, S
Goodloe, A
AF Pike, Lee
Wegmann, Nis
Niller, Sebastian
Goodloe, Alwyn
TI Experience Report: a Do-It-Yourself High-Assurance Compiler
SO ACM SIGPLAN NOTICES
LA English
DT Article
DE Languages; Verification; embedded domain-specific language; compiler;
verification
ID PROGRAMS; TOOL
AB Embedded domain-specific languages (EDSLs) are an approach for quickly building new languages while maintaining the advantages of a rich metalanguage. We argue in this experience report that the "EDSL approach" can surprisingly ease the task of building a high-assurance compiler. We do not strive to build a fully formally-verified tool-chain, but take a "do-it-yourself" approach to increase our confidence in compiler-correctness without too much effort. Copilot is an EDSL developed by Galois, Inc. and the National Institute of Aerospace under contract to NASA for the purpose of runtime monitoring of flight-critical avionics. We report our experience in using type-checking, QuickCheck, and model-checking "off-the-shelf" to quickly increase confidence in our EDSL tool-chain.
C1 [Pike, Lee] Galois Inc, Beaverton, OR USA.
[Wegmann, Nis] Univ Copenhagen, DK-1168 Copenhagen, Denmark.
[Goodloe, Alwyn] NASA, Washington, DC USA.
RP Pike, L (reprint author), Galois Inc, Beaverton, OR USA.
EM leepike@galois.com; niswegmann@gmail.com; sebastian.niller@gmail.com;
a.goodloe@nasa.gov
FU NASA [NNL08AD13T]
FX This work was supported by NASA Contract NNL08AD13T. We wish to
especially thank the following individuals for advice on our work: Ben
Di Vito, Paul Miner, Eric Cooper, Joe Hurd, and Aaron Tomb. Robin
Morisset worked on an earlier version of Copilot. Nis Wegmann and
Sebastian Niller completed this work while they were visiting
researchers at the National Institute of Aerospace.
NR 24
TC 0
Z9 0
U1 1
U2 4
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 0362-1340
J9 ACM SIGPLAN NOTICES
JI ACM Sigplan Not.
PD SEP
PY 2012
VL 47
IS 9
BP 335
EP 340
PG 6
WC Computer Science, Software Engineering
SC Computer Science
GA 040CC
UT WOS:000311296000032
ER
PT J
AU Gottsche, FM
Hulley, GC
AF Goettsche, Frank-M.
Hulley, Glynn C.
TI Validation of six satellite-retrieved land surface emissivity products
over two land cover types in a hyper-arid region
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Land surface emissivity; Hyper-arid region; Emissivity box method;
Generalized split window method; Temperature-emissivity separation;
SEVIRI; ASTER; MODIS
ID THERMAL-INFRARED EMISSIVITIES; ATMOSPHERIC CORRECTION; SEPARATION
ALGORITHM; ASTER TEMPERATURE; BAND; IMAGES; MAPS
AB This study compares six satellite-retrieved land surface emissivity (LSE) products over gravel plains and sand dunes of the hyper-arid Namib desert in Namibia and validates them with in-situ measurements performed with the 'emissivity box method'. The following products are compared: LSE derived by the Land Surface Analysis - Satellite Application Facility (LSA-SAF) for the Spinning Enhanced Visible and Infrared Imager (SEVIRI) onboard Meteosat Second Generation (MSG), LSE products MOD11A2.C5, MOD11B1.C4.1, and MOD11B1.C5 derived for the Moderate Resolution Imaging Spectroradiometer (MODIS) onboard EOS-Terra, LSE derived with the Temperature Emissivity Separation (TES) algorithm for the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) onboard EOS-Terra, and LSE derived with the TES algorithm for EOS-Terra/MODIS data. The LSA-SAF, MOD11A2.C5, and MOD11B1.C5 algorithms directly or indirectly utilize land cover classification and vegetation cover fraction data with the result that for arid regions their LSE are practically identical to the bare ground emissivities assigned to those classes. Over the gravel plains, mean LSA-SAF, ASTER-TES, and MODTES LSE are about 0.950 in the 11 mu m range, whereas mean MOD11A2.C5 and MOD11B1.C5 are about 1.5% (similar to 1 K) higher. The LSA-SAF algorithm misclassifies the sand dunes as 'open & closed shrubland', which results in an overestimated mean LSE (0.969). Since MOD11A2.C5 and MOD11B1.C5 utilize a similar classification and similar emissivity library data, their LSE estimates for the sand dunes are also too high (mean of 0.972 and 0.980, respectively). In contrast, the physics-based ASTER-TES and MODTES algorithms estimate mean sand dune LSE as 0.952 and 0.948, respectively. The physics-based MOD11B1.C4.1 algorithm produced noisy LSE estimates with frequent outliers at 5 km resolution: spatial averaging yielded mean LSE of 0.950 and 0.954 for the gravel plains and the sand dunes, respectively. Based on a combined analysis of in-situ LSE and TES retrieved LSE, and also accounting for uncertainty in the fraction of dry grass (only gravel plains), for future work it is recommended to use SEVIRI ch10.8 emissivities of 0.941 +/- 0.004 for the sand dunes and 0.944 +/- 0.015 for the gravel plains, respectively. The results suggest that split window algorithms would benefit significantly from using physically based MODTES LSE. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Goettsche, Frank-M.] Karlsruhe Inst Technol, D-76344 Eggenstein Leopoldshafen, Germany.
[Hulley, Glynn C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gottsche, FM (reprint author), Karlsruhe Inst Technol, Hermann von Helmholtz Platz 1, D-76344 Eggenstein Leopoldshafen, Germany.
EM frank.goettsche@kit.edu
RI Gottsche, Frank-Michael/A-7362-2013
OI Gottsche, Frank-Michael/0000-0001-5836-5430
FU European Organization for the Exploitation of Meteorological Satellites
(EUMETSAT)
FX This work was carried out within the context of the LSA-SAF project,
funded by the European Organization for the Exploitation of
Meteorological Satellites (EUMETSAT).
NR 46
TC 20
Z9 20
U1 1
U2 29
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2012
VL 124
BP 149
EP 158
DI 10.1016/j.rse.2012.05.010
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700013
ER
PT J
AU Leifer, I
Lehr, WJ
Simecek-Beatty, D
Bradley, E
Clark, R
Dennison, P
Hu, YX
Matheson, S
Jones, CE
Holt, B
Reif, M
Roberts, DA
Svejkovsky, J
Swayze, G
Wozencraft, J
AF Leifer, Ira
Lehr, William J.
Simecek-Beatty, Debra
Bradley, Eliza
Clark, Roger
Dennison, Philip
Hu, Yongxiang
Matheson, Scott
Jones, Cathleen E.
Holt, Benjamin
Reif, Molly
Roberts, Dar A.
Svejkovsky, Jan
Swayze, Gregg
Wozencraft, Jennifer
TI State of the art satellite and airborne marine oil spill remote sensing:
Application to the BP Deepwater Horizon oil spill
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Review
DE Oil spill; Deepwater Horizon; Remote sensing; Lidar; Near infrared;
Thermal infrared; Satellite; Airborne remote sensing; Synthetic aperture
radar; MODIS; Hyperspectral; Multispectral; Expert system; False
positives; Technology readiness; Operational readiness; Visible
spectrum; Oil water emulsions; Spill response; AVIRIS; Synthetic
aperture radar; UAVSAR; Fire; CALIPSO; Oil slick thickness; Laser
fluorescence
ID APERTURE RADAR IMAGERY; SURFACE-FILMS; SEA-SURFACE; HYDROCARBON SEEPS;
PERSIAN-GULF; SAR IMAGES; SLICKS; ALGORITHM; CALIFORNIA; KUWAIT
AB The vast and persistent Deepwater Horizon (DWH) spill challenged response capabilities, which required accurate, quantitative oil assessment at synoptic and operational scales. Although experienced observers are a spill response's mainstay, few trained observers and confounding factors including weather, oil emulsification, and scene illumination geometry present challenges. DWH spill and impact monitoring was aided by extensive airborne and spaceborne passive and active remote sensing.
Oil slick thickness and oil-to-water emulsion ratios are key spill response parameters for containment/cleanup and were derived quantitatively for thick (>0.1 mm) slicks from AVIRIS (Airborne Visible/Infrared Imaging Spectrometer) data using a spectral library approach based on the shape and depth of near infrared spectral absorption features. MODIS (Moderate Resolution Imaging Spectroradiometer) satellite, visible-spectrum broadband data of surface-slick modulation of sunglint reflection allowed extrapolation to the total slick. A multispectral expert system used a neural network approach to provide Rapid Response thickness class maps.
Airborne and satellite synthetic aperture radar (SAR) provides synoptic data under all-sky conditions; however. SAR generally cannot discriminate thick (> 100 mu m) oil slicks from thin sheens (to 0.1 mu m). The UAVSAR's (Uninhabited Aerial Vehicle SAR) significantly greater signal-to-noise ratio and finer spatial resolution allowed successful pattern discrimination related to a combination of oil slick thickness, fractional Surface coverage, and emulsification.
In situ burning and smoke plumes were studied with AVIRIS and corroborated spaceborne CALIPSO (Cloud Aerosol Lidar and Infrared Pathfinder Satellite Observation) observations of combustion aerosols. CALIPSO and bathymetry lidar data documented shallow subsurface oil, although ancillary data were required for confirmation.
Airborne hyperspectral, thermal infrared data have nighttime and overcast collection advantages and were collected as well as MODIS thermal data. However, interpretation challenges and a lack of Rapid Response Products prevented significant use. Rapid Response Products were key to response utilization data needs are time critical; thus, a high technological readiness level is critical to operational use of remote sensing products. DWH's experience demonstrated that development and operationalization of new spill response remote sensing tools must precede the next major oil spill. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Leifer, Ira] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA.
[Lehr, William J.; Simecek-Beatty, Debra] NOAA, Off Response & Restorat, Seattle, WA USA.
[Bradley, Eliza; Roberts, Dar A.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Clark, Roger; Swayze, Gregg] US Geol Survey, Denver, CO 80225 USA.
[Dennison, Philip; Matheson, Scott] Univ Utah, Dept Geog, Salt Lake City, UT USA.
[Dennison, Philip; Matheson, Scott] Univ Utah, Ctr Nat & Technol Hazards, Salt Lake City, UT USA.
[Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Jones, Cathleen E.; Holt, Benjamin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Reif, Molly; Wozencraft, Jennifer] USA, Corp Engineers, Kiln, MS USA.
[Svejkovsky, Jan] Ocean Imaging Corp, Solana Beach, CA USA.
RP Leifer, I (reprint author), Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA.
EM Ira.Leifer@bubbleology.com
RI chen, zhu/K-5923-2013; Hu, Yongxiang/K-4426-2012;
OI Leifer, Ira/0000-0002-4674-5775; Dennison, Philip/0000-0002-0241-1917
FU NASA; NOAA; NSF; USGS; Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration; Bureau of Ocean Energy Management, Regulation, and
Enforcement (BOEMRE) [M07PC13205]
FX We thank the important role and support of NASA, NOAA, NSF, and USGS in
the development of these technologies. Some of the research described
herein was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Development of the multispectral
rapid response thickness sensor by Ocean Imaging was supported by the
Bureau of Ocean Energy Management, Regulation, and Enforcement (BOEMRE)
under contract M07PC13205. NSF support enabled the SEBASS data
collection. The efforts of Susan Ustin (UC Davis) and Raymond Kokaly
(USGS) for ecosystem data collection and analysis and David Tratt for
editing are thanked.
NR 129
TC 103
Z9 112
U1 14
U2 218
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 SEP
PY 2012
VL 124
BP 185
EP 209
DI 10.1016/j.rse.2012.03.024
PG 25
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700016
ER
PT J
AU Geddes, JA
Murphy, JG
O'Brien, JM
Celarier, EA
AF Geddes, Jeffrey A.
Murphy, Jennifer G.
O'Brien, Jason M.
Celarier, Edward A.
TI Biases in long-term NO2 averages inferred from satellite observations
due to cloud selection criteria
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Nitrogen dioxide, NO2; Ground level pollution; Satellite; Ozone
Monitoring Instrument, OMI; Cloud fraction; Remote sensing; Cloud bias;
Toronto; Air quality; Vertical column density
ID OZONE MONITORING INSTRUMENT; GLOBAL DISTRIBUTION; SEASONAL-VARIATIONS;
AIR-QUALITY; IN-SITU; SCIAMACHY; RETRIEVAL; EMISSIONS; SPACE
AB Retrievals of atmospheric trace gas column densities from space are compromised by the presence of clouds, requiring most studies to exclude observations with significant cloud fractions in the instrument's field of view. Using NO2 observations at three ground stations representing urban, suburban, and rural environments, and tropospheric vertical column densities measured by the Ozone Monitoring Instrument (OMI) over each site, we show that the observations from space represent monthly averaged ground-level pollutant conditions well (R = 0.86) under relatively cloud-free conditions. However, by analyzing the ground-level data and applying the OMI cloud fraction as a filter, we show there is a significant bias in long-term averaged NO2 as a result of removing the data during cloudy conditions. For the ground-based sites considered in this study, excluding observations on days when OMI-derived cloud fractions were greater than 0.2 causes 12:00-14:00 mean summer mixing ratios to be underestimated by 12% +/- 6%, 20% +/- 7%, and 40% +/- 10% on average (+/- 1 standard deviation) at the urban, suburban, and rural sites respectively. This bias was investigated in particular at the rural site, a region where pollutant transport is the main source of NO2, and where long-term observations of NOy were also available. Evidence of changing photochemical conditions and a correlation between clear skies and the transport of cleaner air masses play key roles in explaining the bias. The magnitude of a bias is expected to vary from site to site depending on meteorology and proximity to NOx sources, and decreases when longer averaging times of ground station data (e.g. 24-h) are used for the comparison. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Geddes, Jeffrey A.; Murphy, Jennifer G.] Univ Toronto, Dept Chem, Toronto, ON M5S 1A1, Canada.
[O'Brien, Jason M.] Environm Canada, Air Qual Res Div, Toronto, ON, Canada.
[Celarier, Edward A.] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
RP Murphy, JG (reprint author), Univ Toronto, Dept Chem, 80 St George St, Toronto, ON M5S 1A1, Canada.
EM jmurphy@chem.utoronto.ca
RI Geddes, Jeffrey/K-7650-2012; Murphy, Jennifer/C-2367-2011;
OI Geddes, Jeffrey/0000-0001-7573-6133
FU Natural Sciences and Engineering Research Council of Canada
FX Access to air quality monitoring data is provided by the Ontario
Ministry of the Environment We also gratefully acknowledge support from
the Natural Sciences and Engineering Research Council of Canada.
NR 27
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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 SEP
PY 2012
VL 124
BP 210
EP 216
DI 10.1016/j.rse.2012.05.008
PG 7
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700017
ER
PT J
AU Tang, H
Dubayah, R
Swatantran, A
Hofton, M
Sheldon, S
Clark, DB
Blair, B
AF Tang, Hao
Dubayah, Ralph
Swatantran, Anu
Hofton, Michelle
Sheldon, Sage
Clark, David B.
Blair, Bryan
TI Retrieval of vertical LAI profiles over tropical rain forests using
waveform lidar at La Selva, Costa Rica
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE LVIS; Lidar; LAI; Vertical foliage profile; Tropical rain forest;
Geometric Optical and Radiative Transfer; (GORT) model
ID LEAF-AREA INDEX; LARGE-FOOTPRINT LIDAR; CANOPY STRUCTURE; LASER
ALTIMETER; VALIDATION; VEGETATION; BIOMASS; TOPOGRAPHY; FREQUENCY;
PRODUCTS
AB This study explores the potential of waveform lidar in mapping the vertical and spatial distributions of leaf area index (LAI) over the tropical rain forest of La Selva Biological Station in Costa Rica. Vertical profiles of LAI were derived at 0.3 m height intervals from the Laser Vegetation Imaging Sensor (LVIS) data using the Geometric Optical and Radiative Transfer (GORT) model. Cumulative LAI profiles obtained from LVIS were validated with data from 55 ground to canopy vertical transects using a modular field tower to destructively sample all vegetation. Our results showed moderate agreement between lidar and field derived LAI (r(2) = 0.42, RMSE = 1.91, bias = -0.32), which further improved when differences between lidar and tower footprint scales (r(2) = 0.50, RMSE = 1.79, bias = 0.27) and distance of field tower from lidar footprint center (r(2) = 0.63, RMSE = 1.36, bias = 0.0) were accounted for. Next, we mapped the spatial distribution of total LAI across the landscape and analyzed LAI variations over different land cover types. Mean values of total LAI were 1.74, 5.20, 5.41 and 5.62 over open pasture, secondary forests, regeneration forests after selective-logging and old-growth forests respectively. Lastly, we evaluated the sensitivities of our LAI retrieval model to variations in canopy/ground reflectance ratio and to waveform noise such as induced by topographic slopes. We found for both, that the effects were not significant for moderate LAI values (about 4). However model derivations of LAI might be inaccurate in areas of high-slope and high LAI (about 8) if ground return energies are low. This research suggests that large footprint waveform lidar can provide accurate vertical LAI profile estimates that do not saturate even at the high LAI levels in tropical rain forests and may be a useful tool for understanding the light transmittance within these canopies. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Tang, Hao; Dubayah, Ralph; Swatantran, Anu; Hofton, Michelle] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Sheldon, Sage] Univ Oklahoma, Norman, OK 73019 USA.
[Clark, David B.] Univ Missouri, St Louis, MO 63121 USA.
[Blair, Bryan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Tang, H (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
EM htang@umd.edu
RI Blair, James/D-3881-2013; Beckley, Matthew/D-4547-2013; Swatantran,
Anu/B-8786-2016; Tang, Hua/K-4948-2016
OI Tang, Hua/0000-0002-6685-6165
FU NASA's Terrestrial Ecology program [NNX08AP55G]; NSF [0223284]
FX This research was funded by a grant from NASA's Terrestrial Ecology
program (NNX08AP55G). The LAI field data were developed with support
from NSF (0223284). We thank M. Clark for acquiring and processing leaf
and soil spectral data. We also thank W. Ni-Meister for valuable
suggestions on the model.
NR 46
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2012
VL 124
BP 242
EP 250
DI 10.1016/j.rse.2012.05.005
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700021
ER
PT J
AU Lee, CK
Seo, KW
Han, SC
Yu, J
Scambos, TA
AF Lee, Choon-Ki
Seo, Ki-Weon
Han, Shin-Chan
Yu, Jaehyung
Scambos, Ted A.
TI Ice velocity mapping of Ross Ice Shelf, Antarctica by matching surface
undulations measured by ICESat laser altimetry
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Ice velocity; Laser altimetry; Ross Ice Shelf
ID SHEET
AB We present a novel method for estimating the surface horizontal velocity on ice shelves using laser altimetry data from the Ice Cloud and land Elevation Satellite (ICESat; 2003-2009). The method matches undulations measured at crossover points between successive campaigns. Elevation measurements are first relocated into a time-varying (moving) coordinate system using an initial velocity (e.g., from VELMAP), and then crossover height differences are minimized with an adjustment vector. Errors in geolocation of the ICESat tracks result in some error in the adjustment vectors, but these are small relative to the velocity adjustment for fast-moving ice shelves. We use the algorithm to estimate changes in the ice velocity of Ross Ice Shelf between an earlier mapping (from VELMAP) and the ICESat period. The new velocity field is compared with velocities from in situ measurements and satellite radar interferometry. The slowdown of 98 +/- 34 m yr(-1) (similar to 23%) is observed in the ice shelf downstream of Whillans Ice Stream, and the deceleration rate is 3.1 +/- 1.1 m yr(-2) during last three decades. The method can be expanded to the simultaneous mapping of ice horizontal velocity, ice thickness change, and surface deformation for Antarctic ice shelves as well as a more accurate mapping using future ICESat-2 measurements. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Lee, Choon-Ki; Seo, Ki-Weon] Korea Polar Res Inst, Div Polar Earth Syst Sci, Inchon, South Korea.
[Han, Shin-Chan] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Han, Shin-Chan] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Yu, Jaehyung] Chungnam Natl Univ, Dept Geol & Earth Environm Sci, Taejon, South Korea.
[Scambos, Ted A.] Univ Colorado, CIRES, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
RP Lee, CK (reprint author), Korea Polar Res Inst, Div Polar Earth Syst Sci, Inchon, South Korea.
EM cklee92@kopri.re.kr
RI Han, Shin-Chan/A-2022-2009
FU Korea Polar Research Institute (KOPRI) [PE12050]; NASA's Earth Surface
and Interior program; NSF-OPP grant [ANT0732919]
FX The authors thank the Byrd Polar Research Center in Columbus, Ohio, for
providing the InSAR velocity products and L. Padman for providing the
CATS2008a ocean tide model. This work was supported by Korea Polar
Research Institute (KOPRI) projects (PE12050). SCH was supported by
NASA's Earth Surface and Interior program. TAS was supported by NSF-OPP
grant ANT0732919.
NR 26
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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 SEP
PY 2012
VL 124
BP 251
EP 258
DI 10.1016/j.rse.2012.05.017
PG 8
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700022
ER
PT J
AU Chen, G
Wulder, MA
White, JC
Hilker, T
Coops, NC
AF Chen, Gang
Wulder, Michael A.
White, Joanne C.
Hilker, Thomas
Coops, Nicholas C.
TI Lidar calibration and validation for geometric-optical modeling with
Landsat imagery
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Tree height; Landsat; Lidar plots; Li-Strahler geometric-optical model;
Large-area
ID RESOLUTION SATELLITE IMAGERY; SPECTRAL MIXTURE ANALYSIS; CANOPY
REFLECTANCE MODEL; STRUCTURAL-CHANGE DETECTION; FOREST CANOPY; QUICKBIRD
IMAGERY; HEIGHT; VEGETATION; INVENTORY; AIRBORNE
AB There is a paucity of detailed and timely forest inventory information available for Canada's large, remote northern boreal forests. The Canadian National Forest Inventory program has derived a limited set of attributes from a Landsat-based land cover product representing circa year 2000 conditions. Of the required inventory attributes, forest vertical structure (e.g., tree height) is critical for terrestrial biomass and carbon modeling and to date, is unavailable for these remote areas. In this study, we develop a large-area, fine-scale (25 m) mapping solution to estimate tree height (mean, dominant, and Lorey's height) across Canada's northern forests by integrating lidar data (representing 0.27% of the study area), and Landsat imagery (representing 100% of the study area), using a geometric-optical modeling technique. First, spectral mixture analysis (SMA) was used to extract image endmembers and generate fraction images. Second, lidar data were used to calibrate the inverted geometric-optical model by adjusting the model's three key fractional inputs: sunlit crown, sunlit background, and shade fraction, based upon the SMA derived images. The heterogeneity of the study area, spanning 2.16 million ha, made it challenging to directly and accurately decompose mixed Landsat image pixels into the canopy and background fractions used for the Li-Strahler geometric-optical model inversion. As a result we developed a novel method to use the lidar plot data to facilitate the calculation of these fractions in an accurate and automated manner. The average estimation errors for mean, dominant, and Lorey's height were 4.9 m, 4.1 m, and 4.7 m, respectively when compared to the lidar data, with the best result achieved using dominant tree height, where the average error was 3.5 m for over 80% of the forested area. Using this approach of optical remotely sensed data calibrated and validated with lidar height estimates, we generate and evaluate wall-to-wall estimates of tree height that can subsequently be used as inputs for biomass and carbon modeling. Crown Copyright (C) 2012 Published by Elsevier Inc. All rights reserved.
C1 [Chen, Gang; Wulder, Michael A.; White, Joanne C.] Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC V8Z 1M5, Canada.
[Hilker, Thomas] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Coops, Nicholas C.] Univ British Columbia, Fac Forestry, Dept Forest Resources Management, Integrated Remote Sensing Studio, Vancouver, BC V6T 1Z4, Canada.
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 Coops, Nicholas/J-1543-2012; Wulder, Michael/J-5597-2016;
OI Coops, Nicholas/0000-0002-0151-9037; Wulder,
Michael/0000-0002-6942-1896; White, Joanne/0000-0003-4674-0373
FU Natural Sciences and Engineering Research Council (NSERC); Canadian
Space Agency (CSA), Government Related Initiatives Program (GRIP);
Canadian Forest Service (CFS) of Natural Resources Canada
FX This research has been funded by a Natural Sciences and Engineering
Research Council (NSERC) Visiting Fellowship award to Dr. Gang Chen.
Aspects of this research were undertaken as part of the "EcoMonitor:
Northern Ecosystem Climate Change Monitoring" project jointly funded by
the Canadian Space Agency (CSA), Government Related Initiatives Program
(GRIP) and the Canadian Forest Service (CFS) of Natural Resources
Canada.
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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 SEP
PY 2012
VL 124
BP 384
EP 393
DI 10.1016/j.rse.2012.05.026
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700033
ER
PT J
AU Cheng, YB
Middleton, EM
Zhang, QY
Corp, LA
Dandois, J
Kustas, WP
AF Cheng, Yen-Ben
Middleton, Elizabeth M.
Zhang, Qingyuan
Corp, Lawrence A.
Dandois, Jonathan
Kustas, William P.
TI The photochemical reflectance index from directional cornfield
reflectances: Observations and simulations
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Hyperspectral; Two-layer Analytical Canopy Reflectance; Model (ACRM);
Photochemical reflectance index (PRI); Cornfield
ID LIGHT-USE-EFFICIENCY; RADIATION-USE-EFFICIENCY; NET PRIMARY PRODUCTION;
LEAF PIGMENT CONTENT; CANOPY REFLECTANCE; SPECTRAL REFLECTANCE; CO2
UPTAKE; PHOTOSYNTHETIC EFFICIENCY; XANTHOPHYLL CYCLE; DATA ASSIMILATION
AB The two-layer Markov chain Analytical Canopy Reflectance Model (ACRM) was linked with in situ hyperspectral leaf optical properties to simulate the Photochemical Reflectance Index (PRI) for a corn crop canopy at three different growth stages. This is an extended study after a successful demonstration of PRI simulations for a cornfield previously conducted at an early vegetative growth stage. Consistent with previous in situ studies, sunlit leaves exhibited lower PRI values than shaded leaves. Since sunlit (shaded) foliage dominates the canopy in the reflectance hotspot (coldspot), the canopy PRI derived from field hyperspectral observations displayed sensitivity to both view zenith angle and relative azimuth angle at all growth stages. Consequently, sunlit and shaded canopy sectors were most differentiated when viewed along the azimuth matching the solar principal plane. These directional PRI responses associated with sunlit/shaded foliage were successfully reproduced by the ACRM. As before, the simulated PRI values from the current study were closer to in situ values when both sunlit and shaded leaves were utilized as model input data in a two-layer mode, instead of a one-layer mode with sunlit leaves only. Model performance as judged by correlation between in situ and simulated values was strongest for the mature corn crop (r = 0.87, RMSE = 0.0048), followed by the early vegetative stage (r = 0.78; RMSE = 0.0051) and the early senescent stage (r = 0.65; RMSE = 0.0104). Since the benefit of including shaded leaves in the scheme varied across different growth stages, a further analysis was conducted to investigate how variable fractions of sunlit/shaded leaves affect the canopy PRI values expected for a cornfield, with implications for remote sensing monitoring options. Simulations of the sunlit to shaded canopy ratio near 50/50 +/- 10 (e.g., 60/40) matching field observations at all growth stages were examined. Our results suggest the importance of the sunlit/shaded fraction and canopy structure in understanding and interpreting PRI. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Cheng, Yen-Ben; Middleton, Elizabeth M.] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cheng, Yen-Ben] Earth Resources Technol Inc, Laurel, MD 20707 USA.
[Zhang, Qingyuan] Unvers Space Res Assoc, Columbia, MD 21044 USA.
[Corp, Lawrence A.] Sigma Space Corp, Lanham, MD 20706 USA.
[Dandois, Jonathan] Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, Baltimore, MD 21250 USA.
[Kustas, William P.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
RP Cheng, YB (reprint author), NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA.
EM Yen-Ben.Cheng@nasa.gov
RI Kustas, William/C-2063-2015
FU NASA ROSES project through Carbon Cycle Science Program
FX This study was supported by a NASA ROSES project (PI, E.M. Middleton)
funded through the Carbon Cycle Science Program (Diane Wickland,
manager). The authors gratefully acknowledge A. Kuusk for sharing
computer code for the canopy reflectance model, and K.F. Huemmrich
(UMBC), P.K.E. Campbell (UMBC), A. Russ (USDA-ARS Hydrology and Remote
Sensing Lab) and D. Lagomasino (FIU) for assisting field campaign and
their valuable comments. The authors thank the anonymous reviewers for
their very valuable suggestions and criticism.
NR 69
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SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2012
VL 124
BP 444
EP 453
DI 10.1016/j.rse.2012.05.030
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700038
ER
PT J
AU Asner, GP
Knapp, DE
Boardman, J
Green, RO
Kennedy-Bowdoin, T
Eastwood, M
Martin, RE
Anderson, C
Field, CB
AF Asner, Gregory P.
Knapp, David E.
Boardman, Joseph
Green, Robert O.
Kennedy-Bowdoin, Ty
Eastwood, Michael
Martin, Roberta E.
Anderson, Christopher
Field, Christopher B.
TI Carnegie Airborne Observatory-2: Increasing science data dimensionality
via high-fidelity multi-sensor fusion
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Airborne remote sensing; CAO; Data fusion; Hyperspectral; Imaging
spectroscopy; LiDAR, Light detection and ranging; Macroscale ecology
ID IMAGING SPECTROMETER DATA; HUMID TROPICAL FORESTS; SMALL-FOOTPRINT
LIDAR; RAIN-FOREST; HYPERSPECTRAL DISCRIMINATION; CLIMATE-CHANGE;
WATER-VAPOR; CANOPY; SPECTROSCOPY; VEGETATION
AB The Carnegie Airborne Observatory (CAO) was developed to address a need for macroscale measurements that reveal the structural, functional and organismic composition of Earth's ecosystems. In 2011, we completed and launched the CAO-2 next generation Airborne Taxonomic Mapping Systems (AToMS), which includes a high-fidelity visible-to-shortwave infrared (VSWIR) imaging spectrometer (380-2510 nm), dual-laser waveform light detection and ranging (LiDAR) scanner, and high spatial resolution visible-to-near infrared (VNIR) imaging spectrometer (365-1052 nm). Here, we describe how multiple data streams from these sensors can be fused using hardware and software co-alignment and processing techniques. With these data streams, we quantitatively demonstrate that precision data fusion greatly increases the dimensionality of the ecological information derived from remote sensing. We compare the data dimensionality of two contrasting scenes - a built environment at Stanford University and a lowland tropical forest in Amazonia. Principal components analysis revealed 336 dimensions (degrees of freedom) in the Stanford case, and 218 dimensions in the Amazon. The Amazon case presents what could be the highest level of remotely sensed data dimensionality ever reported for a forested ecosystem. Simulated misalignment of data streams reduced the effective information content by up to 48%, highlighting the critical role of achieving high precision when undertaking multi-sensor fusion. The instrumentation and methods described here are a pathfinder for future airborne applications undertaken by the National Ecological Observatory Network (NEON) and other organizations. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Asner, Gregory P.; Knapp, David E.; Boardman, Joseph; Kennedy-Bowdoin, Ty; Martin, Roberta E.; Anderson, Christopher; Field, Christopher B.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Boardman, Joseph] Analyt Imaging & Geophys LLC, Boulder, CO 80303 USA.
[Green, Robert O.; Eastwood, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Asner, GP (reprint author), Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA.
EM gpa@stanford.edu
RI Asner, Gregory/G-9268-2013
OI Asner, Gregory/0000-0001-7893-6421
FU Gordon and Betty Moore Foundation; John D. and Catherine T. MacArthur
Foundation; Grantham Foundation for the Protection of the Environment;
W.M. Keck Foundation; William Hearst III
FX The Carnegie Airborne Observatory is supported by the Gordon and Betty
Moore Foundation, the John D. and Catherine T. MacArthur Foundation, the
Grantham Foundation for the Protection of the Environment, the W.M. Keck
Foundation, and William Hearst III.
NR 75
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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 SEP
PY 2012
VL 124
BP 454
EP 465
DI 10.1016/j.rse.2012.06.012
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700039
ER
PT J
AU Veraverbeke, S
Hook, SJ
Harris, S
AF Veraverbeke, S.
Hook, S. J.
Harris, S.
TI Synergy of VSWIR (0.4-2.5 mu m) and MTIR (3.5-12.5 mu m) data for
post-fire assessments
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Fire severity; Multiple Endmember Spectral Mixture Analysis (MESMA);
Wildfire emission; Carbon; Differenced Normalized Burn Ratio (dNBR);
Burn severity; Char; Charcoal; Spectral unmixing
ID SPECTRAL MIXTURE ANALYSIS; NORMALIZED BURN RATIO; DIFFERENCE VEGETATION
INDEX; 2007 PELOPONNESE WILDFIRES; ESTIMATING FIRE SEVERITY; LANDSAT
THEMATIC MAPPER; REMOTELY-SENSED DATA; BOREAL FORESTS; TIME-SERIES;
REFLECTANCE
AB Post-fire effects assessments are crucial to evaluate the impact of fire on ecosystems. They are helpful in planning post-fire rehabilitation and useful for reducing uncertainties in current wildfire emission estimates. We have used MODIS/ASTER (MASTER) airborne simulator data over the 2011 Canyon fire in California, USA to evaluate the potential synergy between visible to short-wave infrared (VSWIR, 0.4-2.5 mu m) and mid to thermal infrared (MTIR, 3.5-12.5 mu m) data in a post-fire environment. We applied Multiple Endmember Spectral Mixture Analysis (MESMA) inputting five endmembers: char, green vegetation, non-photosynthetic vegetation (NPV), substrate and shadow. Results revealed that fractional cover estimates of char, NPV and substrate are 5-7% better when VSWIR-MTIR data were combined, compared to using only VSWIR data. Combined VSWIR-MTIR imagery will become available at pixel sizes smaller than 100 m with future satellite sensors, such as the Hyperspectral Infrared Imager (HyspIRI). The MESMA-derived char fractional cover was also shown to be strongly correlated with the Geo Composite Burn Index (GeoCBI, R-adj(2) = 0.82) and the percentage of black trees and shrubs (R-adj(2) = 0.66) measured in the field. SMA-derived char fractions provide quantitative abundance maps which should prove valuable for improving wildfire emission estimates by refining burning efficiency values. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Veraverbeke, S.; Hook, S. J.; Harris, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Harris, S.] Monash Univ, Sch Geog & Environm Sci, Melbourne, Vic 3800, Australia.
RP Veraverbeke, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sander.S.Veraverbeke@jpl.nasa.gov; Simon.J.Hook@jpl.nasa.gov;
sarah.harris@monash.edu
RI Veraverbeke, Sander/H-2301-2012
OI Veraverbeke, Sander/0000-0003-1362-5125
FU NASA
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. The
work was funded by a NASA grant for Interdisciplinary Research in Earth
Science awarded to Dr. Yufang Jin. We would like to thank the anonymous
reviewers for their useful suggestions to improve the manuscript.
Copyright 2012 California Institute of Technology. Government
sponsorship acknowledged.
NR 73
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PU ELSEVIER SCIENCE INC
PI NEW YORK
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SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2012
VL 124
BP 771
EP 779
DI 10.1016/j.rse.2012.06.028
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 039LQ
UT WOS:000311247700064
ER
PT J
AU de Val-Borro, M
Hartogh, P
Jarchow, C
Rengel, M
Villanueva, GL
Kuppers, M
Biver, N
Bockelee-Morvan, D
Crovisier, J
AF de Val-Borro, M.
Hartogh, P.
Jarchow, C.
Rengel, M.
Villanueva, G. L.
Kueppers, M.
Biver, N.
Bockelee-Morvan, D.
Crovisier, J.
TI Submillimetric spectroscopic observations of volatiles in comet C/2004
Q2 (Machholz)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: individual: C/2004 Q2 (Machholz); molecular processes; radiative
transfer; techniques: spectroscopic; submillimeter: planetary systems
ID CHIRP TRANSFORM SPECTROMETER; BOPP C/1995 O1; HALE-BOPP; WATER-VAPOR;
MOLECULAR-SPECTROSCOPY; RADIATIVE-TRANSFER; RADIO OBSERVATIONS; LINE
OBSERVATIONS; COLOGNE DATABASE; PARENT VOLATILES
AB Context: Submillimeter spectroscopic observations of comets provide an important tool for understanding their chemical composition and enable a taxonomic classification.
Aims. We aim to determine the production rates of several parent- and product volatiles and the C-12/C-13 isotopic carbon ratio in the long-period comet C/2004 Q2 (Machholz), which is likely to originate from the Oort Cloud.
Methods. The line emission from several molecules in the coma was measured with high signal-to-noise ratio in January 2005 at heliocentric distance of 1.2 AU by means of high-resolution spectroscopic observations using the Submillimeter Telescope (SMT) at the Arizona Radio Observatory (ARO).
Results. We have obtained production rates of several volatiles (CH3OH, HCN, (HCN)-C-13, HNC, H2CO, CO, and CS) by comparing the observed and simulated line-integrated intensities. We calculated the synthetic profiles using a radiative transfer code that includes collisions between neutrals and electrons, and the effects of radiative pumping of the fundamental vibrational levels by solar infrared radiation. Furthermore, multiline observations of the CH3OH J = 7-6 series allow us to estimate the rotational temperature using the rotation diagram technique. We find that the CH3OH population distribution of the levels sampled by these lines can be described by a rotational temperature of 40 +/- 3 K. Derived mixing ratios relative to hydrogen cyanide are CO/CH3OH/H2CO/CS/HNC/H13CN/HCN = 30.9/24.6/4.8/0.57/0.031/0.013/1 assuming a pointing offset of 8 '' due to the uncertain ephemeris at the time of the observations and the telescope pointing error.
Conclusions. The measured relative molecular abundances in C/2004 Q2 (Machholz) are between low- to typical values of those obtained in Oort Cloud comets, suggesting that it has visited the inner solar system previously and undergone thermal processing. The HNC/HCN abundance ratio of similar to 3.1% is comparable to that found in other comets, accounting for the dependence on the heliocentric distance, and could possibly be explained by ion-molecule chemical processes in the low-temperature atmosphere. From a tentative (HCN)-C-13 detection, the measured value of 97 +/- 30 for the (HCN)-C-12/(HCN)-C-13 isotopologue pair is consistent with a telluric value. The outgassing variability observed in the HCN production rates over a period of two hours is consistent with the rotation of the nucleus derived using different observational techniques.
C1 [de Val-Borro, M.; Hartogh, P.; Jarchow, C.; Rengel, M.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Villanueva, G. L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Villanueva, G. L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Kueppers, M.] European Space Agcy, European Space Astron Ctr, Rosetta Sci Operat Ctr, Madrid 28691, Spain.
[Biver, N.; Bockelee-Morvan, D.; Crovisier, J.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92195 Meudon, France.
RP de Val-Borro, M (reprint author), Max Planck Inst Solar Syst Res, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM deval@mps.mpg.de; hartogh@mps.mpg.de; jarchow@mps.mpg.de;
rengel@mps.mpg.de; geronimo.villanueva@nasa.gov;
michael.kueppers@sciops.esa.int; nicolas.biver@obspm.fr;
dominique.bockelee@obspm.fr; jacques.crovisier@obspm.fr
RI de Val-Borro, Miguel/H-1319-2013
OI de Val-Borro, Miguel/0000-0002-0455-9384
FU Special Priority Program 1488 of the German Science Foundation
FX The SMT is operated by the Arizona Radio Observatory (ARO), Steward
Observatory, University of Arizona. We are grateful to the ARO staff for
their support during these observations. This work was supported by the
Special Priority Program 1488 of the German Science Foundation. M.dV.B.
acknowledges fruitful discussions with Michal Drahus during the course
of this work. We thank the referee, Michael F. A'Hearn, for helpful
comments that improved the manuscript.
NR 86
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2012
VL 545
AR A2
DI 10.1051/0004-6361/201219172
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012RT
UT WOS:000309254900002
ER
PT J
AU Haberl, F
Sturm, R
Ballet, J
Bomans, DJ
Buckley, DAH
Coe, MJ
Corbet, R
Ehle, M
Filipovic, MD
Gilfanov, M
Hatzidimitriou, D
La Palombara, N
Mereghetti, S
Pietsch, W
Snowden, S
Tiengo, A
AF Haberl, F.
Sturm, R.
Ballet, J.
Bomans, D. J.
Buckley, D. A. H.
Coe, M. J.
Corbet, R.
Ehle, M.
Filipovic, M. D.
Gilfanov, M.
Hatzidimitriou, D.
La Palombara, N.
Mereghetti, S.
Pietsch, W.
Snowden, S.
Tiengo, A.
TI The XMM-Newton survey of the Small Magellanic Cloud
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Magellanic Clouds; ISM: supernova remnants; X-rays: ISM
ID X-RAY SOURCES; CHANDRA ACIS SURVEY; GALACTIC SUPERNOVA-REMNANTS; HOT
INTERSTELLAR-MEDIUM; PHOTON IMAGING CAMERA; ATCA RADIO-CONTINUUM; ROSAT
PSPC CATALOG; CLASSICAL NOVAE; CENTRAL REGION; OPTICAL NOVAE
AB Context. Although numerous archival XMM-Newton observations existed towards the Small Magellanic Cloud (SMC) before 2009, only a fraction of the whole galaxy had been covered.
Aims. Between May 2009 and March 2010, we carried out an XMM-Newton survey of the SMC, to ensure a complete coverage of both its bar and wing. Thirty-three observations of 30 different fields with a total exposure of about one Ms filled the previously missing parts.
Methods. We systematically processed all available SMC data from the European Photon Imaging Camera. After rejecting observations with very high background, we included 53 archival and the 33 survey observations. We produced images in five different energy bands. We applied astrometric boresight corrections using secure identifications of X-ray sources and combined all the images to produce a mosaic covering the main body of the SMC.
Results. We present an overview of the XMM-Newton observations, describe their analysis, and summarise our first results, which will be presented in detail in follow-up papers. Here, we mainly focus on extended X-ray sources, such as supernova remnants (SNRs) and clusters of galaxies, that are seen in our X-ray images.
Conclusions. Our XMM-Newton survey represents the deepest complete survey of the SMC in the 0.15-12.0 keV X-ray band. We propose three new SNRs that have low surface brightnesses of a few 10(-14) erg cm(-2) s(-1) arcmin(-2) and large extents. In addition, several known remnants appear larger than previously measured at either X-rays or other wavelengths extending the size distribution of SMC SNRs to larger values.
C1 [Haberl, F.; Sturm, R.; Pietsch, W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Ballet, J.] Univ Paris Diderot, Lab AIM, CEA Saclay, CEA,DSM,CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France.
[Bomans, D. J.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany.
[Buckley, D. A. H.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Coe, M. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Corbet, R.] Univ Maryland Baltimore Cty, Xray Astrophys Lab, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ehle, M.] ESA, ESAC, XMM Newton Sci Operat Ctr, Madrid 28691, Spain.
[Filipovic, M. D.] Univ Western Sydney, Penrith, NSW 1797, Australia.
[Gilfanov, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Hatzidimitriou, D.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
[La Palombara, N.; Mereghetti, S.; Tiengo, A.] Ist Astrofis Spaziale & Fis Cosm Milano, INAF, I-20133 Milan, Italy.
[Snowden, S.] NASA, High Energy Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.
[Tiengo, A.] Ist Univ Studi Super Pavia, I-27100 Pavia, Italy.
RP Haberl, F (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM fwh@mpe.mpg.de
RI Hatzidimitriou, Despina/A-3732-2015;
OI La Palombara, Nicola/0000-0001-7015-6359; Haberl,
Frank/0000-0002-0107-5237; Tiengo, Andrea/0000-0002-6038-1090;
MEREGHETTI, SANDRO/0000-0003-3259-7801
FU ESA Member states; USA (NASA); Bundesministerium fur Wirtschaft und
Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR) [FKZ 50
OX 0001]; Max-Planck Society; NSF [AST-9540747, AST-0307613]; University
of Michigan; BMWI/DLR [FKZ 50 OR 0907]; Italian Space Agency through
ASI/INAF [I/009/10/0, I/032/10/0]
FX Based on observations with XMM-Newton, an ESA Science Mission with
instruments and contributions directly funded by ESA Member states and
the USA (NASA).; The XMM-Newton project is supported by the
Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur
Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OX 0001) and the Max-Planck
Society. The Magellanic Clouds Emission Line Survey (MCELS) data were
provided by R. C. Smith, P. F. Winkler, and S. D. Points. The MCELS
project has been supported in part by NSF grants AST-9540747 and
AST-0307613, and through the generous support of the Dean B. McLaughlin
Fund at the University of Michigan, a bequest from the family of Dr.
Dean B. McLaughlin in memory of his lasting impact on Astronomy. The
National Optical Astronomy Observatory is operated by the Association of
Universities for Research in Astronomy Inc. (AURA), under a cooperative
agreement with the National Science Foundation. R. Sturm acknowledges
support from the BMWI/DLR, FKZ 50 OR 0907. N. La Palombara, S. L.
Mereghetti and A. Tiengo acknowledge financial contributions by the
Italian Space Agency through ASI/INAF agreements I/009/10/0 and
I/032/10/0 for data analysis and XMM-Newton operations, respectively.
NR 60
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2012
VL 545
AR A128
DI 10.1051/0004-6361/201219758
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012RT
UT WOS:000309254900128
ER
PT J
AU Pierbattista, M
Grenier, IA
Harding, AK
Gonthier, PL
AF Pierbattista, M.
Grenier, I. A.
Harding, A. K.
Gonthier, P. L.
TI Constraining gamma-ray pulsar gap models with a simulated pulsar
population
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: neutron; pulsars: general; gamma rays: stars; radiation
mechanisms: non-thermal; methods: numerical; surveys
ID HIGH-ENERGY EMISSION; LARGE-AREA TELESCOPE; RADIO PULSARS; MILLISECOND
PULSARS; FREQUENCY SURVEY; POWERED PULSARS; GALACTIC PLANE; LIGHT
CURVES; POLAR CAPS; SLOT GAPS
AB With the large sample of young gamma-ray pulsars discovered by the Fermi Large Area Telescope (LAT), population synthesis has become a powerful tool for comparing their collective properties with model predictions. We synthesised a pulsar population based on a radio emission model and four gamma-ray gap models (Polar Cap, Slot Gap, Outer Gap, and One Pole Caustic). Applying gamma-ray and radio visibility criteria, we normalise the simulation to the number of detected radio pulsars by a select group of ten radio surveys. The luminosity and the wide beams from the outer gaps can easily account for the number of Fermi detections in 2 years of observations. The wide slot-gap beam requires an increase by a factor of similar to 10 of the predicted luminosity to produce a reasonable number of gamma-ray pulsars. Such large increases in the luminosity may be accommodated by implementing offset polar caps. The narrow polar-cap beams contribute at most only a handful of LAT pulsars. Using standard distributions in birth location and pulsar spin-down power ((E) over dot), we skew the initial magnetic field and period distributions in a an attempt to account for the high (E) over dot Fermi pulsars. While we compromise the agreement between simulated and detected distributions of radio pulsars, the simulations fail to reproduce the LAT findings: all models under-predict the number of LAT pulsars with high (E) over dot, and they cannot explain the high probability of detecting both the radio and gamma-ray beams at high (E) over dot. The beaming factor remains close to 1.0 over 4 decades in (E) over dot evolution for the slot gap whereas it significantly decreases with increasing age for the outer gaps. The evolution of the enhanced slot-gap luminosity with (E) over dot is compatible with the large dispersion of gamma-ray luminosity seen in the LAT data. The stronger evolution predicted for the outer gap, which is linked to the polar cap heating by the return current, is apparently not supported by the LAT data. The LAT sample of gamma-ray pulsars therefore provides a fresh perspective on the early evolution of the luminosity and beam width of the gamma-ray emission from young pulsars, calling for thin and more luminous gaps.
C1 [Pierbattista, M.; Grenier, I. A.] Univ Paris Diderot, CEA IRFU CNRS, CEA Saclay, Labo AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Pierbattista, M.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Francois Arago Ctr,Observ Paris,APC, F-75205 Paris 13, France.
[Grenier, I. A.] Inst Univ France, Paris, France.
[Harding, A. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Gonthier, P. L.] Hope Coll, Dept Phys, Holland, MI 49423 USA.
RP Pierbattista, M (reprint author), Univ Paris Diderot, CEA IRFU CNRS, CEA Saclay, Labo AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
EM marco.pierbattista@cea.fr
FU NASA Astrophysics Theory program; Fermi GI program; NSF under the RUI
program
FX M.P. acknowledges Patrizia Caraveo and the IASF-INAF of Milan for the
hospitality and help, thanks Damien Parent for the helpful suggestions,
and acknowledges Volker Beckmann and the Francois Arago Centre for
hospitality. M.P. acknowledges P and Isabel Caballero for the help.
A.K.H. and P.L.G. acknowledges support from the NASA Astrophysics Theory
and Fermi GI programs. P.L.G. also appreciates the support from NSF
under the RUI program. We acknowledge the referee for the useful
suggestions.
NR 63
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FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2012
VL 545
AR A42
DI 10.1051/0004-6361/201219135
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012RT
UT WOS:000309254900042
ER
PT J
AU Podio, L
Kamp, I
Flower, D
Howard, C
Sandell, G
Mora, A
Aresu, G
Brittain, S
Dent, WRF
Pinte, C
White, GJ
AF Podio, L.
Kamp, I.
Flower, D.
Howard, C.
Sandell, G.
Mora, A.
Aresu, G.
Brittain, S.
Dent, W. R. F.
Pinte, C.
White, G. J.
TI Herschel/PACS observations of young sources in Taurus: the far-infrared
counterpart of optical jets
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrochemistry; stars: formation; ISM: jets and outflows; ISM:
molecules; ISM: general
ID HUBBLE-SPACE-TELESCOPE; DRIVEN MOLECULAR OUTFLOW; HERBIG-HARO OBJECTS;
MASS-LOSS RATES; T-TAURI; DARK CLOUD; DG-TAURI; ADAPTIVE OPTICS;
ACCRETION RATES; DISK ACCRETION
AB Context. Observations of the atomic and molecular line emission associated with jets and outflows emitted by young stellar objects provide sensitive diagnostics of the excitation conditions, and can be used to trace the various evolutionary stages they pass through as they evolve to become main sequence stars.
Aims. To understand the relevance of atomic and molecular cooling in shocks, and how accretion and ejection efficiency evolves with the evolutionary state of the sources, we will study the far-infrared counterparts of bright optical jets associated with Class I and II sources in Taurus (T Tau, DG Tau A, DG Tau B, FS Tau A + B, and RW Aur).
Methods. We have analysed Herschel/PACS observations of a number of atomic ([OI]63 mu m, 145 mu m, [C II]158 mu m) and molecular (high-J CO, H2O, OH) lines, collected within the open time key project GASPS (PI: W. R. F. Dent). To constrain the origin of the detected lines we have compared the obtained FIR emission maps with the emission from optical-jets and millimetre-outflows, and the measured line fluxes and ratios with predictions from shock and disk models.
Results. All of the targets are associated with extended emission in the atomic lines; in particular, the strong [OI] 63 mu m emission is correlated with the direction of the optical jet/mm-outflow. The line ratios suggest that the atomic lines can be excited in fast dissociative J-shocks occurring along the jet. The molecular emission, on the contrary, originates from a compact region, that is spatially and spectrally unresolved, and lines from highly excited levels are detected (e.g., the o-H(2)O8(18)-7(07) line, and the CO J = 36-35 line). Disk models are unable to explain the brightness of the observed lines (CO and H2O line fluxes up to 10(-15)-6 x 10(-16) W m(-2)). Slow C- or J-shocks with high pre-shock densities reproduce the observed H2O and high-J CO lines; however, the disk and/or UV-heated outflow cavities may contribute to the observed emission.
Conclusions. Similarly to Class 0 sources, the FIR emission associated with Class I and II jet-sources is likely to be shock-excited. While the cooling is dominated by CO and H2O lines in Class 0 sources, [OI] becomes an important coolant as the source evolves and the environment is cleared. The cooling and mass loss rates estimated for Class II and I sources are one to four orders of magnitude lower than for Class 0 sources. This provides strong evidence to indicate that the outflow activity decreases as the source evolves.
C1 [Podio, L.] Inst Planetol & Astrophys Grenoble, F-38400 St Martin Dheres, France.
[Podio, L.; Kamp, I.] Univ Groningen, Kapteyn Inst, NL-9747 AD Groningen, Netherlands.
[Flower, D.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Howard, C.; Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Washington, DC USA.
[Mora, A.] ESA, ESAC Gaia SOC, Madrid 28691, Spain.
[Brittain, S.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Dent, W. R. F.] ALMA, Santiago, Chile.
[White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[White, G. J.] Rutherford Appleton Lab, RALSpace, Didcot OX11 0QX, Oxon, England.
RP Podio, L (reprint author), Inst Planetol & Astrophys Grenoble, 414 Rue Piscine, F-38400 St Martin Dheres, France.
EM podio@obs.ujf-grenoble.fr
FU FP7 Intra-European Marie Curie Fellowship [PIEF-GA-2009-253896]; NWO
MEERVOUD grant
FX L. Podio acknowledges the funding from the FP7 Intra-European Marie
Curie Fellowship (PIEF-GA-2009-253896). C. Howard, G. Sandell, and S.
Brittain acknowledge NASA/JPL. I. Kamp acknowledges funding from an NWO
MEERVOUD grant. We thank the PACS instrument team for their dedicated
support. We also thank J. Eisloffel for letting us use the images
published in Eisloffel & Mundt (1998) for the plots in Fig. 2. Finally
we are grateful to B. Nisini, C. Codella, A. Karska and the referee for
very useful discussion and comments that helped improving the paper.
NR 89
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2012
VL 545
AR A44
DI 10.1051/0004-6361/201219475
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012RT
UT WOS:000309254900044
ER
PT J
AU Riaud, P
Mawet, D
Magette, A
AF Riaud, P.
Mawet, D.
Magette, A.
TI Nijboer-Zernike phase retrieval for high contrast imaging Principle,
on-sky demonstration with NACO, and perspectives in vector vortex
coronagraphy
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: high angular resolution; instrumentation: adaptive
optics; methods: numerical; techniques: polarimetric
AB We introduce a novel phase retrieval method for astronomical applications based on the Nijboer-Zernike (NZ) theory of diffraction. We present a generalized NZ phase retrieval process that is not limited to small and symmetric aberrations and can therefore be directly applied to astronomical imaging instruments. We describe a practical demonstration of this novel method that was recently performed using data taken on-sky with NAOS-CONICA, the adaptive optics system of the Very Large Telescope. This demonstration presents the first online on-sky phase retrieval results ever obtained, and allows us to plan subsequent refinements on a well-tested basis. Among the potential refinements, and within the framework of high-contrast imaging of extra-solar planetary systems (which requires exquisite wavefront quality), we introduce an extension of the generalized NZ to the high-dynamic range case, and particularly to its use with the vector vortex coronagraph. This induces conjugated phase ramps applied to the orthogonal circular polarizations, which can be used to instantaneously retrieve the complex amplitude of the field, yielding a real-time calibration of the wavefront that does not need any other modulation such as focus or other deformable mirror probe patterns. Paper II (Riaud et al. 2012, A&A, 545, A151) presents the mathematical and practical details of the new method.
C1 [Riaud, P.; Magette, A.] Univ Liege, B-4000 Sart Tilman Par Liege, Belgium.
[Mawet, D.] European So Observ, Santiago 3107, Chile.
[Mawet, D.] NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA.
[Magette, A.] Techspace Aero, B-4041 Milmort, Belgium.
RP Riaud, P (reprint author), 60 Rue bergers, F-75015 Paris, France.
EM riaud.pierre@gmail.com; dmawet@eso.org; arnaud.magette@techspace-aero.be
FU University of Liege; Communaute francaise de Belgique - Actions de
recherche concertees - Academie universitaire Wallonie-Europe
FX This work received the support of the University of Liege. The authors
are grateful to C. Hanot (IAGL), and J. Surdej (IAGL) for the manuscript
corrections. The authors wish to thank the referee Wesley Traub for
useful comments and corrections. The authors also acknowledge support
from the Communaute francaise de Belgique - Actions de recherche
concertees - Academie universitaire Wallonie-Europe. This idea dates
back to 2005-2006 and the first author is grateful to Sect. 17 and the
CNAP French commissions for their outstanding recruitment work.
NR 11
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2012
VL 545
AR A150
DI 10.1051/0004-6361/201219613
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012RT
UT WOS:000309254900150
ER
PT J
AU Riaud, P
Mawet, D
Magette, A
AF Riaud, P.
Mawet, D.
Magette, A.
TI Instantaneous phase retrieval with the vector vortex coronagraph
Theoretical and optical implementation
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: high angular resolution; instrumentation: adaptive
optics; methods: numerical; techniques: polarimetric
ID MASK CORONAGRAPH; DIVERSITY
AB Coronagraphs are used as high-contrast imaging tools. However, it is well-known that the achievable contrast is primarily limited by wavefront aberrations in the optical train. Various kinds of devices and methods have been proposed to correct and calibrate these errors and, hence, improve the efficiency of coronagraphs. Here, we present an innovative idea that allows instantaneous measuring of the phase and the amplitude of residual stellar speckles in coronagraphic images. The technique is based on the unique polarization properties of the vector vortex coronagraph, which serves as a new type of phase diversity (POAM diversity), as well an extension of the Nijboer-Zernike theory of aberrations. We also propose and discuss a simple practical optical implementation of the technique, which only requires polarization splitting at the back-end of any existing vector vortex coronagraph systems.
C1 [Riaud, P.; Magette, A.] Univ Liege, B-4000 Sart Tilman Par Liege, Belgium.
[Mawet, D.] European So Observ, Santiago 19, Chile.
[Mawet, D.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Magette, A.] Techspace Aero, B-4041 Milmort, Belgium.
RP Riaud, P (reprint author), 60 Rue Bergers, F-75084 Paris, France.
EM riaud.pierre@gmail.com; dmawet@eso.org; magette@techspace-aero.be
FU University of Liege; Communaute francaise de Belgique - Actions de
recherche concertees - Academie universitaire Wallonie-Europe
FX This work received the support of the University of Liege. This work was
partly carried out at the European Southern Observatory (ESO) site of
Vitacura (Santiago, Chile). The authors are grateful to C. Hanot (IAGL),
D. Defrere (MPI-RA) for manuscript corrections. The authors wish to
thank the referee Wesley Traub for his useful comments and corrections.
The authors also acknowledge support from the Communaute francaise de
Belgique - Actions de recherche concertees - Academie universitaire
Wallonie-Europe. This idea dates back to 2005-2006 and the first author
is grateful to section 17 and the CNAP French commissions for their
outstanding recruitment work.
NR 26
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2012
VL 545
AR A151
DI 10.1051/0004-6361/201219614
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 012RT
UT WOS:000309254900151
ER
PT J
AU Chen, NY
Sridhar, B
Ng, HK
AF Chen, Neil Y.
Sridhar, Banavar
Ng, Hok K.
TI Tradeoff Between Contrail Reduction and Emissions in United States
National Airspace
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation and Control Conference
CY AUG 02-06, 2010
CL Toronto, CANADA
SP Amer Inst Aeronaut & Astronaut (AIAA)
ID CLIMATE-CHANGE; IMPACTS; CIRRUS; AVIATION; COVERAGE
AB This paper describes a class of strategies for reducing persistent contrail formation with the capability of trading off between contrails and aircraft-induced emissions. The concept of contrail-frequency index is defined and used to quantify the contrail activities. The contrail-reduction strategies reduce the contrail-frequency index by altering aircraft's cruising altitude with consideration to extra emissions. The strategies use a user-defined factor to trade off between contrail reduction and extra emissions. The analysis shows that contrails can be reduced with extra emissions and without adding congestion to airspace. For a day with high contrail activities, the results show that the maximal contrail-reduction strategy can achieve a contrail reduction of 88%. When a tradeoff factor is used, the strategy can achieve less contrail reduction while emitting less emissions compared to the maximal contrail-reduction strategy. The user-defined tradeoff factor provides a flexible way to trade off between contrail reduction and extra emissions. Better understanding of the tradeoffs between contrails and emissions and their impact on the climate need to be developed to fully use this class of contrail-reduction strategies. The strategies provide a starting point for developing operational policies to reduce the impact of aviation on climate.
C1 [Chen, Neil Y.] NASA, Ames Res Ctr, Syst Modeling & Optimizat Branch, Moffett Field, CA 94035 USA.
[Sridhar, Banavar] NASA, Ames Res Ctr, Aviat Syst Div, Moffett Field, CA 94035 USA.
[Ng, Hok K.] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, Moffett Field, CA 94035 USA.
RP Chen, NY (reprint author), NASA, Ames Res Ctr, Syst Modeling & Optimizat Branch, MS 210-10, Moffett Field, CA 94035 USA.
NR 27
TC 1
Z9 1
U1 3
U2 4
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 1367
EP 1375
DI 10.2514/1.C031680
PG 9
WC Engineering, Aerospace
SC Engineering
GA 019JQ
UT WOS:000309736200018
ER
PT J
AU Miller, SG
Lort, RD
Zimmerman, TJ
Sutter, JK
Pelham, LI
McCorkle, LS
Scheiman, DA
AF Miller, S. G.
Lort, R. D., III
Zimmerman, T. J.
Sutter, J. K.
Pelham, L. I.
McCorkle, L. S.
Scheiman, D. A.
TI Face-Sheet Quality Analysis and Thermo-Physical Property
Characterization of OOA and Autoclave Panels
SO SAMPE JOURNAL
LA English
DT Article
AB Increased application of polymer matrix composite (PMC) materials in large vehicle structures requires consideration of non-autoclave manufacturing technology. The NASA Composites for Exploration project, and its predecessor Lightweight Spacecraft Structures and Materials project, were tasked with the development of materials and manufacturing processes for structures that will perform in a heavy-lift-launch vehicle environment. Both autoclave and out-of-autoclave processable materials were considered. Large PMC structures envisioned for such a vehicle included the payload shroud and the interstage connector In this study, composite sandwich panels representing 1/16th segments of the barrel section of the Ares V rocket fairing were prepared as 1.8 m x 2.4 vi sections of the 10 m diameter arc segment. 1M7/977-3 was used as the face-sheet prepreg of the autoclave processed panels and T40-800B/5320-1 for the out-of-autoclave panels. The core was 49.7 kg/m(2) (3.1 lb/ft(3) (pcf)) aluminum honeycomb. Face-sheets were fabricated by automated tape laying 153 mm wide unidirectional tape. This work details analysis of the manufactured panels where face-sheet quality was characterized by optical microscopy, cured ply thickness measurements, acid digestion, and thermal analysis.
C1 [Miller, S. G.; Sutter, J. K.] NASA Glenn Res Ctr, Cleveland, OH USA.
[Lort, R. D., III; Zimmerman, T. J.] BG Smith & Associates, Huntsville, AL USA.
[Pelham, L. I.] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
[McCorkle, L. S.] Ohio Aerosp Inst, Cleveland, OH USA.
[Scheiman, D. A.] ASRC Aerosp Corp, Cleveland, OH USA.
RP Miller, SG (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA.
NR 5
TC 1
Z9 1
U1 0
U2 7
PU SAMPE PUBLISHERS
PI COVINA
PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA
SN 0091-1062
J9 SAMPE J
JI Sampe J.
PD SEP-OCT
PY 2012
VL 48
IS 5
BP 56
EP 61
PG 6
WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 991ZW
UT WOS:000307745400004
ER
PT J
AU Anderson, HR
Butland, BK
van Donkelaar, A
Brauer, M
Strachan, DP
Clayton, T
van Dingenen, R
Amann, M
Brunekreef, B
Cohen, A
Dentener, F
Lai, C
Lamsal, LN
Martin, RV
AF Anderson, H. Ross
Butland, Barbara K.
van Donkelaar, Aaron
Brauer, Michael
Strachan, David P.
Clayton, Tadd
van Dingenen, Rita
Amann, Marcus
Brunekreef, Bert
Cohen, Aaron
Dentener, Frank
Lai, Christopher
Lamsal, Lok N.
Martin, Randall V.
CA ISAAC Phase One Study Grp
ISAAC Phase Three Study Grp
TI Satellite-based Estimates of Ambient Air Pollution and Global Variations
in Childhood Asthma Prevalence
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Article
DE air pollution; asthma prevalence; children; epidemiology; global;
nitrogen dioxide; ozone; particulate matter; satellite observations
ID PARTICULATE POLLUTION; MODEL TM5; ISAAC; ALLERGIES; AEROSOL; MORTALITY;
SYMPTOMS; EXPOSURE; CHILDREN
AB BACKGROUND: The effect of ambient air pollution on global variations and trends in asthma prevalence is unclear.
OBJECTIVES: Our goal was to investigate community-level associations between asthma prevalence data from the International Study of Asthma and Allergies in Childhood (ISAAC) and satellite-based estimates of particulate matter with aerodynamic diameter < 2.5 mu m (PM2.5) and nitrogen dioxide (NO2), and modelled estimates of ozone.
METHODS: We assigned satellite-based estimates of PM2.5 and NO2 at a spatial resolution of 0.1 degrees x 0.1 degrees and modeled estimates of ozone at a resolution of 1 degrees x 1 degrees to 183 ISAAC centers. We used center-level prevalence of severe asthma as the outcome and multilevel models to adjust for gross national income (GM) and center- and country-level sex, climate, and population density. We examined associations (adjusting for GNI) between air pollution and asthma prevalence over time in centers with data from ISAAC Phase One (mid-1900s) and Phase Three (2001-2003).
RESULTS: For the 13- to 14-year age group (128 centers in 28 countries), the estimated average within-country change in center-level asthma prevalence per 100 children per 10% increase in center-level PM2.5 and NO2 was -0.043 [95% confidence interval (Cl): 0.139, 0.053] and 0.017 (95% Cl: 0.030, 0.064) respectively. For ozone the estimated change in prevalence per parts per billion by volume was -0.116 (95% Cl: -0.234, 0.001). Equivalent results for the 6- to 7-year age group (83 centers in 20 countries), though slightly different, were not significantly positive. For the 13- to 14-year age group, change in center-level asthma prevalence over time per 100 children per 10% increase in PM2.5 from Phase One to Phase Three was -0.139 (95% Cl: -0.347, 0.068). The corresponding association with ozone (per ppbV) was -0.171(95% Cl: -0.275, -0.067).
CONCLUSION: In contrast to reports from within-community studies of individuals exposed to traffic pollution, we did not find evidence of a positive association between ambient air pollution and asthma prevalence as measured at the community level.
C1 [Anderson, H. Ross] Univ London, Div Populat Hlth Sci & Educ, MRC HPA Ctr Environm & Hlth, London SW17 0RE, England.
[Anderson, H. Ross] Kings Coll London, MRC HPA Ctr Environm & Hlth, London, England.
[Brauer, Michael] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
[van Donkelaar, Aaron; Lamsal, Lok N.; Martin, Randall V.] Dalhousie Univ, Halifax, NS, Canada.
[Clayton, Tadd] Univ Auckland, Auckland 1, New Zealand.
[van Dingenen, Rita; Dentener, Frank] Commiss European Communities, Joint Res Ctr, I-21020 Ispra, Italy.
[Amann, Marcus] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria.
[Brunekreef, Bert] Inst Risk Assessment Sci, Utrecht, Netherlands.
[Brunekreef, Bert] Julius Ctr Hlth Sci & Primary Care, Utrecht, Netherlands.
[Cohen, Aaron] Hlth Effects Inst, Boston, MA USA.
[Lai, Christopher] Chinese Univ Hong Kong, Hong Kong, Hong Kong, Peoples R China.
[Lamsal, Lok N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Lamsal, Lok N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Anderson, HR (reprint author), Univ London, Div Populat Hlth Sci & Educ, MRC HPA Ctr Environm & Hlth, Cranmer Terrace, London SW17 0RE, England.
EM r.anderson@sgul.ac.uk
RI Lamsal, Lok/G-4781-2012; Martin, Randall/C-1205-2014; Ellwood,
Philippa/G-7555-2015;
OI Martin, Randall/0000-0003-2632-8402; Ellwood,
Philippa/0000-0002-1994-4023; brunekreef, bert/0000-0001-9908-0060;
Brauer, Michael/0000-0002-9103-9343
FU ISAAC; U.S. Environmental Protection Agency; worldwide motor industry
FX We thank the children and parents who participated in ISAAC Phase One
and Phase Three, the school staff for their assistance and help with
coordination, the ISAAC principal investigators and their colleagues,
and the many funding bodies throughout the world that supported the
individual ISAAC centers and collaborators and their meetings. We also
thank M. Field-Smith for her assistance with the preparation of this
paper. All investigators in the Phase One and Phase Three study groups
are listed in Supplemental Material, p. 3.; M.A. is employed by the
International Institute for Applied Systems Analysis, Austria. A.C. is
employed by the Health Effects Institute (HEI), Boston, MA, USA. The HEI
receives about half of its core funds from the U.S. Environmental
Protection Agency and half from the worldwide motor industry. The views
expressed in this paper are those of the authors and do not necessarily
reflect the views of the HEI or its sponsors.
NR 36
TC 25
Z9 26
U1 3
U2 40
PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE
PI RES TRIANGLE PK
PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233,
RES TRIANGLE PK, NC 27709-2233 USA
SN 0091-6765
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD SEP
PY 2012
VL 120
IS 9
BP 1333
EP 1339
DI 10.1289/ehp.1104724
PG 7
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA 005YV
UT WOS:000308786900034
PM 22548921
ER
PT J
AU Jensen, BD
Bandyopadhyay, A
Wise, KE
Odegard, GM
AF Jensen, Benjamin D.
Bandyopadhyay, Ananyo
Wise, Kristopher E.
Odegard, Gregory M.
TI Parametric Study of ReaxFF Simulation Parameters for Molecular Dynamics
Modeling of Reactive Carbon Gases
SO JOURNAL OF CHEMICAL THEORY AND COMPUTATION
LA English
DT Article
ID FORCE-FIELD; THERMAL-DECOMPOSITION; GROWTH; DIAMOND; HYDROGEN;
FULLERENES; PRECURSORS; NANOTUBES; CLUSTER; OXYGEN
AB The development of innovative carbon-based materials can be greatly facilitated by molecular modeling techniques. Although the Reax Force Field (ReaxFF) can be used to simulate the chemical behavior of carbon-based systems, the simulation settings required for accurate predictions have not been fully explored. Using the ReaxFF, molecular dynamics (MD) simulations are used to simulate the chemical behavior of pure carbon and hydrocarbon reactive gases that are involved in the formation of carbon structures such as graphite, buckyballs, amorphous carbon, and carbon nanotubes. It is determined that the maximum simulation time step that can be used in MD simulations with the ReaxFF is dependent on the simulated temperature and selected parameter set, as are the predicted reaction rates. It is also determined that different carbon-based reactive gases react at different rates, and that the predicted equilibrium structures are generally the same for the different ReaxFF parameter sets, except in the case of the predicted formation of large graphitic structures with the Chenoweth parameter set under specific conditions.
C1 [Jensen, Benjamin D.; Bandyopadhyay, Ananyo; Odegard, Gregory M.] Michigan Technol Univ, Dept Mech Engn Engn Mech, Houghton, MI 49931 USA.
[Wise, Kristopher E.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Odegard, GM (reprint author), Michigan Technol Univ, Dept Mech Engn Engn Mech, Houghton, MI 49931 USA.
EM gmodegar@mtu.edu
RI Jensen, Benjamin/B-1297-2013;
OI Jensen, Benjamin/0000-0002-7982-0663; Odegard,
Gregory/0000-0001-7577-6565
FU NASA under the Revolutionary Technology Challenges Program [NNX09AM50A]
FX This research was funded by NASA under the Revolutionary Technology
Challenges Program (Grant No. NNX09AM50A).
NR 29
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U1 2
U2 50
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 SEP
PY 2012
VL 8
IS 9
BP 3003
EP 3008
DI 10.1021/ct300491d
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 006PG
UT WOS:000308830700004
PM 26605713
ER
PT J
AU Yu, SS
Pearson, JC
Drouin, BJ
Martin-Drumel, MA
Pirali, O
Vervloet, M
Coudert, LH
Muller, HSP
Brunken, S
AF Yu, Shanshan
Pearson, John C.
Drouin, Brian J.
Martin-Drumel, Marie-Aline
Pirali, Olivier
Vervloet, Michel
Coudert, Laurent H.
Mueller, Holger S. P.
Bruenken, Sandra
TI Measurement and analysis of new terahertz and far-infrared spectra of
high temperature water
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE High temperature water; THz spectroscopy; FIR spectroscopy; RF
discharge; DC discharge; Anomalous centrifugal distortion
ID ABSOLUTE FREQUENCY MEASUREMENT; EXCITED VIBRATIONAL-STATE; BACKWARD-WAVE
OSCILLATORS; POTENTIAL-ENERGY SURFACE; BROAD-BAND SPECTROSCOPY; LINE
INTENSITY ANALYSES; LYING ROTATIONAL LEVELS; VAPOR LASER TRANSITION;
LAMB-DIP TECHNIQUE; HYPERFINE-STRUCTURE
AB Terahertz absorption spectroscopy and far infrared Fourier transform (FIR-FT) emission spectroscopy were employed to measure new rotational and ro-vibrational spectra and validate existing datasets for high temperature water, with the goal to improve the accuracy of predictions for pure rotation in the (0 2 0), (1 0 0) and (0 0 1) vibrational states. A total of 104 new rotational transitions in (0 0 0), (0 1 0), (0 2 0), (1 0 0) and (0 0 1) were observed in the 293-2723 GHz region with MW accuracy and with observed J(Max) = 18, 11, 10, 14, 10; K-a(Max)= 10, 7, 7, 7, 4; E ''(Max)= 4178, 3771, 4996, 5430, 4939 cm(-1), respectively. A total of 4194 new FIR-FT transitions were assigned in the 50-600 cm(-1) region to the same five vibrational states with estimated experimental uncertainty of 0.0008-0.002 cm(-1) and with J(Max) = 27; K-a(Max) = 21, 18, 18, 17, 17, respectively. Together with previous high-resolution observations, these new data were fitted with the Bending-Rotation approach and the Euler Hamiltonian. The new measurements and predictions reported here will support the analyses of astronomical observations by high-resolution spectroscopy telescopes such as Herschel, SOFIA, and ALMA. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Yu, Shanshan; Pearson, John C.; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Martin-Drumel, Marie-Aline; Pirali, Olivier] Univ Paris 11, CNRS, Inst Sci Mol ISMO, F-91405 Orsay, France.
[Martin-Drumel, Marie-Aline; Pirali, Olivier; Vervloet, Michel] SOLEIL Synchrotron, F-91192 Gif Sur Yvette, France.
[Coudert, Laurent H.] Univ Paris Est Creteil, CNRS, Lab Interuniv Syst Atmospher, UMR 7583, F-94010 Creteil, France.
[Coudert, Laurent H.] Univ Paris Diderot, F-94010 Creteil, France.
[Mueller, Holger S. P.; Bruenken, Sandra] 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 Brunken, Sandra/B-1880-2010; Yu, Shanshan/D-8733-2016;
OI Brunken, Sandra/0000-0001-7175-4828; Mueller,
Holger/0000-0002-0183-8927; Martin-Drumel,
Marie-Aline/0000-0002-5460-4294
FU National Aeronautics and Space Administration; Deutsche
Forschungsgemeinschaft (DFG) [SFB 494]; Bundesministerium fur Bildung
und Forschung (BMBF) [FKZ 50OF0901]
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. HSPM and SB acknowledge
initial support by the Deutsche Forschungsgemeinschaft (DFG) via the
collaborative research grant SFB 494. HSPM is also very grateful to the
Bundesministerium fur Bildung und Forschung (BMBF) for more recent
financial support through Project FKZ 50OF0901 (ICC HIFI Herschel). We
would like to thank the reviewer for useful suggestions and J. Tennyson
and L. Lodi for providing us with the CVR and LTP2011 linelists for the
comparison of line intensities.
NR 94
TC 14
Z9 14
U1 0
U2 32
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD SEP
PY 2012
VL 279
BP 16
EP 25
DI 10.1016/j.jms.2012.07.011
PG 10
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 024KO
UT WOS:000310108300004
ER
PT J
AU Nguyen, H
Cressie, N
Braverman, A
AF Hai Nguyen
Cressie, Noel
Braverman, Amy
TI Spatial Statistical Data Fusion for Remote Sensing Applications
SO JOURNAL OF THE AMERICAN STATISTICAL ASSOCIATION
LA English
DT Article
DE Aerosol optical depth; Fixed rank kriging; Geostatistics; Prediction
standard error
ID NUMERICAL-MODELS; AEROSOL; INTERPOLATION; SATELLITE; MISR
AB Aerosols are tiny solid or liquid particles suspended in the atmosphere; examples of aerosols include windblown dust, sea salts, volcanic ash, smoke from wildfires, and pollution from factories. The global distribution of aerosols is a topic of great interest in climate studies since aerosols can either cool or warm the atmosphere depending on their location, type, and interaction with clouds. Aerosol concentrations are important input components of global climate models, and it is crucial to accurately estimate aerosol concentrations from remote sensing instruments so as to minimize errors "downstream" in climate models. Currently, space-based observations of aerosols are available from two remote sensing instruments on board NASA's Terra spacecraft: the Mu Wangle Imaging SpectroRadiometer (MISR), and the MODerate-resolution Imaging Spectrometer (MODIS). These two instruments have complementary coverage, spatial support, and retrieval characteristics, making it advantageous to combine information from both sources to make optimal inferences about global aerosol distributions.
In this article, we predict the true aerosol process from two noisy and possibly biased datasets, and we also estimate the uncertainties of these estimates. Our data-fusion methodology scales linearly and bears some resemblance to Fixed Rank Kriging (FRK), a variant of kriging that is designed for spatial interpolation of a single, massive dataset. Our spatial statistical approach does not require assumptions of stationarity or isotropy and, crucially, allows for change of spatial support. We compare our methodology to FRK and Bayesian melding, and we show that ours has superior prediction standard errors compared to FRK and much faster computational speed compared to Bayesian melding.
C1 [Hai Nguyen; Braverman, Amy] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Cressie, Noel] Ohio State Univ, Program Spatial Stat & Environm Stat, Columbus, OH 43210 USA.
[Cressie, Noel] Ohio State Univ, Dept Stat, Columbus, OH 43210 USA.
RP Nguyen, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM hai.nguyen@jpl.nasa.gov; ncressie@stat.osu.edu;
Amy.J.Bravennan@jpl.nasa.gov
RI Cressie, Noel/B-8858-2009
OI Cressie, Noel/0000-0002-0274-8050
FU NASA; NASA's Earth Science Technology Office through its Advanced
Information Systems Technology program
FX Hai Nguyen is Statistician, Jet Propulsion Laboratory, California
Institute of Technology, Pasadena, CA 91125 (E-mail:
hai.nguyen@jpl.nasa.gov). Noel Cressie is Director of the Program in
Spatial Statistics and Environmental Statistics and Distinguished
Professor, Department of Statistics, The Ohio State University,
Columbus, OH 43210 (E-mail: ncressie@stat.osu.edu). Amy Braverman is
Senior Statistician, Jet Propulsion Laboratory, California Institute of
Technology, Pasadena, CA 91125 (E-mail: Amy.J.Braverman@jpl.nasa.gov).
The research described in this article began as part of Nguyen's PhD
dissertation in the Department of Statistics at UCLA, and was continued
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with NASA. It is supported by NASA's Earth Science
Technology Office through its Advanced Information Systems Technology
program. We would like to express our appreciation for all comments
received during the review process.
NR 34
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U1 7
U2 48
PU AMER STATISTICAL ASSOC
PI ALEXANDRIA
PA 732 N WASHINGTON ST, ALEXANDRIA, VA 22314-1943 USA
SN 0162-1459
J9 J AM STAT ASSOC
JI J. Am. Stat. Assoc.
PD SEP
PY 2012
VL 107
IS 499
BP 1004
EP 1018
DI 10.1080/01621459.2012.694717
PG 15
WC Statistics & Probability
SC Mathematics
GA 020FC
UT WOS:000309793400015
ER
PT J
AU Matson, DL
Castillo-Rogez, JC
Davies, AG
Johnson, TV
AF Matson, Dennis L.
Castillo-Rogez, Julie C.
Davies, Ashley Gerard
Johnson, Torrence V.
TI Enceladus: A hypothesis for bringing both heat and chemicals to the
surface
SO ICARUS
LA English
DT Article
DE Enceladus; Geological processes; Geophysics; Interiors
ID E-RING; SATURNS RINGS; LIQUID WATER; SALT-WATER; PLUME; OCEAN;
FRACTURES; STABILITY; ERUPTIONS; MODELS
AB The eruptive plumes and large heat flow (similar to 15 GW) observed by Cassini in the South Polar Region of Enceladus may be expressions of hydrothermal activity inside Enceladus. We hypothesize that a subsurface ocean is the heat reservoir for thermal anomalies on the surface and the source of heat and chemicals necessary for the plumes. The ocean is believed to contain dissolved gases, mostly CO2 and is found to be relatively warm (similar to 0 degrees C). Regular tidal forces open cracks in the icy crust above the ocean. Ocean water fills these fissures. There, the conditions are met for the upward movement of water and the dissolved gases to exsolve and form bubbles, lowering the bulk density of the water column and making the pressure at its bottom less than that at the top of the ocean. This pressure difference drives ocean water into and up the conduits toward the surface. This transportation mechanism supports the thermal anomalies and delivers heat and chemicals to the chambers from which the plumes erupt. Water enters these chambers and there its bubbles pop and loft an aerosol mist into the ullage. The exiting plume gas entrains some of these small droplets. Thus, nonvolatile chemical species in ocean water can be present in the plume particles. A CO2 equivalent-gas molar fraction of similar to 4 x 10(-4) for the ocean is sufficient to support the circulation. A source of heat is needed to keep the ocean warm at similar to 0 degrees C (about two degrees above its freezing point). The source of heat is unknown, but our hypothesis is not dependent on any particular mechanism for producing the heat. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Matson, Dennis L.; Castillo-Rogez, Julie C.; Davies, Ashley Gerard; Johnson, Torrence V.] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
RP Matson, DL (reprint author), CALTECH, Jet Prop Lab, Mail Code 183-301,4800 Oak Grove Dr, Pasadena, CA 91101 USA.
EM dmatson@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This paper has benefited very much from two reviews, especially from
Dave Stevenson. Jonathan Lunine was a participant in early phases of
this work and we are grateful for his insights and ongoing interest.
This work has been conducted at the Jet Propulsion Laboratory,
California Institute of Technology under a contract with the National
Aeronautics and Space Administration. Copyright 2012 California
Institute of Technology. All rights reserved. Government sponsorship
acknowledged.
NR 55
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U1 5
U2 41
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 53
EP 62
DI 10.1016/j.icarus.2012.05.031
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200005
ER
PT J
AU Neish, CD
Prockter, LM
Patterson, GW
AF Neish, C. D.
Prockter, L. M.
Patterson, G. W.
TI Observational constraints on the identification and distribution of
chaotic terrain on icy satellites
SO ICARUS
LA English
DT Article
DE Europa; Triton; Image processing
ID EUROPA; STATE; SELECTION; MECHANISM; EVOLUTION; HISTORY; TRITON; SHELL;
WATER
AB We outline the observational constraints required to identify chaos regions on Europa. Large incidence angle, rather than high resolution, appears to be the primary observational requirement for identifying chaos. At incidence angles >70 degrees, chaos can be identified on Europa at image resolutions as low as 1.5 km/pixel. Similar images obtained at moderate or low incidence angles (<50 degrees) require image resolutions upwards of similar to 250 m/pixel to identify chaos. If global images of Europa can be acquired at high incidence angles, the majority of its chaotic terrain can be identified, helping to constrain models of chaos formation and distribution. Furthermore, our results indicate that the areal coverage of chaos may be more uncertain than previously reported, representing as little as 10% or as much as 50% of the non-polar regions of Europa. These guidelines will aid in the development of optical instruments for future Europa missions, as well as other icy bodies, such as Triton. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Neish, C. D.; Prockter, L. M.; Patterson, G. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Neish, CD (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM catherine.d.neish@nasa.gov
RI Neish, Catherine/G-6321-2012; Patterson, Gerald/E-7699-2015
FU NASA [NNH07ZDA001N-OPR]
FX We thank Tammy Becker at the USGS for her help in constructing the E17
regional mosaic, and two anonymous reviewers for their constructive
comments. This work was supported by the NASA NNH07ZDA001N-OPR program
grant to L.P.
NR 25
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U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 72
EP 79
DI 10.1016/j.icarus.2012.07.009
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200007
ER
PT J
AU Poppe, AR
Piquette, M
Likhanskii, A
Horanyi, M
AF Poppe, Andrew R.
Piquette, Marcus
Likhanskii, Alexandre
Horanyi, Mihaly
TI The effect of surface topography on the lunar photoelectron sheath and
electrostatic dust transport
SO ICARUS
LA English
DT Article
DE Moon, Surface; Asteroids, Surface; Regoliths
ID PONDED DEPOSITS; CHARGED DUST; LEVITATION; PLASMA; EROS; TERMINATOR;
ASTEROIDS; DYNAMICS; 433-EROS; FORCES
AB The dayside near-surface lunar plasma environment is electrostatically complex, due to the interaction between solar UV-induced photoemission, the collection of ambient ions and electrons, and the presence of micron and sub-micron sized dust grains. Further complicating this environment, although less well understood in effect, is the presence of surface relief, typically in the form of craters and/or boulders. It has been suggested that such non-trivial surface topography can lead to complex electrostatic potentials and fields, including "mini-wakes" behind small obstacles to the solar wind flow and "supercharging" near sunlit-shadowed boundaries (Criswell, D.R., De, B.R. [1977]. J. Geophys. Res. 82 (7); De, BR., Criswell, D.R. [1977]. J. Geophys. Res. 82(7): Farrell, W.M., Stubbs, T.J., Vondrak, R.R., Delory, G.T., Halekas, J.S. [2007]. Geophys. Res. Lett. 34; Wang, X., Horanyi, M., Sternovsky, Z., Robertson, S., Morfill, G.E. [2007]. Geophys. Res. Lett. 34, L16104). In this paper, we present results from a three-dimensional, self-consistent, electrostatic particle-in-cell code used to model the dayside near-surface lunar plasma environment over a variety of local times with the presence of a crater. Additionally, we use the particle-in-cell model output to study the effect of surface topography on the dynamics of electrostatic dust transport, with the goal of understanding previous observations of dust dynamics on the Moon and dust ponding on various asteroids. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Poppe, Andrew R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Piquette, Marcus; Horanyi, Mihaly] Univ Colorado, Colorado Ctr Lunar Dust & Atmospher Studies, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Likhanskii, Alexandre] Tech X Corp, Boulder, CO 80303 USA.
[Horanyi, Mihaly] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Poppe, Andrew R.; Horanyi, Mihaly] NASA, Lunar Sci Inst, Mountain View, CA 94089 USA.
RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM poppe@ssl.berkeley.edu
OI Poppe, Andrew/0000-0001-8137-8176; Horanyi, Mihaly/0000-0002-5920-9226
FU NASA Lunar Science Institute through the Colorado Center for Lunar Dust
and Atmospheric Studies [NNX08AY77G]; NASA Earth and Space Science
Graduate Fellowship [NNX08BA17H]; NASA Lunar Science Institute through
the Dynamic Response of the Environment at the Moon (DREAM) team
FX The authors thank the NASA Lunar Science Institute for their support
through the Colorado Center for Lunar Dust and Atmospheric Studies,
Grant #NNX08AY77G. A.R.P. gratefully acknowledges support from a NASA
Earth and Space Science Graduate Fellowship, Grant #NNX08BA17H, and from
the NASA Lunar Science Institute through the Dynamic Response of the
Environment at the Moon (DREAM) team. The authors also thank P. Messmer
for useful discussions in designing the simulation model and two
anonymous reviewers from helpful and constructive comments.
NR 52
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 135
EP 146
DI 10.1016/j.icarus.2012.07.018
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200012
ER
PT J
AU Gaier, JR
AF Gaier, James R.
TI Interpretation of the Apollo 14 Thermal Degradation Sample experiment
SO ICARUS
LA English
DT Article
DE Moon, Surface; Moon; Solar wind
AB The Thermal Degradation Sample (TDS) experiment was one of the many investigations performed on the lunar surface during Apollo 14. Remarkably, the results of this 40 year old experiment were never fully interpreted, perhaps in part because the hardware vanished after its return. Mission records, high resolution photographs returned from the mission, and recent laboratory investigations have been used to glean important results from this experiment. It is most likely that the dust adhesion to the TDS was less than anticipated because of atomic-level contamination of its surfaces. These contaminants were probably removed from most equipment surfaces on the Moon by sputter cleaning by the solar wind, but the TDS experiments were not exposed to the solar wind long enough to affect the cleaning. Published by Elsevier Inc.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Gaier, JR (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM James.R.Gaier@nasa.gov
NR 20
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 167
EP 173
DI 10.1016/j.icarus.2012.07.002
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200015
ER
PT J
AU Fougere, N
Combi, MR
Tenishev, V
Rubin, M
Bonev, BP
Mumma, MJ
AF Fougere, N.
Combi, M. R.
Tenishev, V.
Rubin, M.
Bonev, B. P.
Mumma, M. J.
TI Understanding measured water rotational temperatures and column
densities in the very innermost coma of Comet 73P/Schwassmann-Wachmann 3
B
SO ICARUS
LA English
DT Article
DE Comets; Comets, Coma; Infrared observations; Atmospheres, Dynamics
ID RADIATIVE-TRANSFER; GRIGG-SKJELLERUP; MODEL; DUST; GAS; P/HALLEY;
SIMULATION; CHEMISTRY; HALLEY; IONS
AB Direct sublimation of a comet nucleus surface is usually considered to be the main source of gas in the coma of a comet. However, evidence from a number of comets including the recent spectacular images of Comet 103P/Hartley 2 by the EPOXI mission indicates that the nucleus alone may not be responsible for all, or possibly at times even most, of the total amount of gas seen in the coma. Indeed, the sublimation of icy grains, which have been injected into the coma, appears to constitute an important source. We use the fully-kinetic Direct Simulation Monte Carlo model of Tenishev et al. (Tenishev, V.M., Combi, M.R., Davidsson, B. [2008]. Astrophys. J., 685, 659-677; Tenishev, V.M., Combi, M.R., Rubin, M. [2011]. Astrophys. J., 732) to reproduce the measurements of column density and rotational temperature of water in Comet 73P-B/Schwassmann-Wachmann 3 obtained with a very high spatial resolution of similar to 30 km using IRCS/Subaru in May 2006 (Bonev, B.P., Mumma, M.J., Kawakita, H., Kobayashi, H., Villanueva, G.L. [2008]. Icarus, 196, 241-248). For gas released solely from the cometary nucleus at a heliocentric distance of 1 AU, modeled rotational temperatures start at 110 K close to the surface and decrease to only several tens of degrees by 10-20 nucleus radii. However, the measured decay of both rotational temperature and column density with distance from the nucleus is much slower than predicted by this simple model. The addition of a substantial (distributed) source of gas from icy grains in the model slows the decay in rotational temperature and provides a more gradual drop in column density profiles. Together with a contribution of rotational heating of water molecules by electrons, the combined effects allow a much better match to the IRCS/Subaru observations. From the spatial distributions of water abundance and temperature measured in 73P/SW3-B, we have identified and quantified multiple mechanisms of release. The application of this tool to other comets may permit such studies over a range of heliocentric and geocentric distances. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Fougere, N.; Combi, M. R.; Tenishev, V.; Rubin, M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Bonev, B. P.; Mumma, M. J.] NASA, Goddard Ctr Astrobiol, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fougere, N (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM fougere@umich.edu
RI Combi, Michael/J-1697-2012; Tenishev, Valeriy/B-7658-2013; mumma,
michael/I-2764-2013; Rubin, Martin/I-7777-2013
OI Combi, Michael/0000-0002-9805-0078; Rubin, Martin/0000-0001-6549-3318
FU NASA [NNX09AB59G]; JPL under NASA [1266313, 1266314, NMO710889]; NSF
Astronomy and Astrophysics Research Grants Programs [AST-0807939]; NASA
Astrobiology Institute [RTOP 344-53-51]; NASA Planetary Astronomy
Program [RTOP 344-32-07]
FX We are grateful to Dr. Geronimo Villanueva for useful discussions on
accounting on the comparison between modeled and observed column
densities and rotational temperatures. This work was supported by NASA
Planetary Atmospheres Grant NNX09AB59G, and JPL Subcontracts 1266313 and
1266314 under NASA Grant NMO710889 to the U.S. Rosetta Project. The
computations were made with NAS computer resources at NASA Ames under
GID 26135. B.P.B. acknowledges support from the NSF Astronomy and
Astrophysics Research Grants Programs (AST-0807939). M.J.M. acknowledges
support from the NASA Astrobiology Institute (RTOP 344-53-51) and
Planetary Astronomy Program (RTOP 344-32-07).
NR 64
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 174
EP 185
DI 10.1016/j.icarus.2012.07.019
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200016
ER
PT J
AU Boyce, JM
Wilson, L
Mouginis-Mark, PJ
Hamilton, CW
Tornabene, LL
AF Boyce, Joseph M.
Wilson, Lionel
Mouginis-Mark, Peter J.
Hamilton, Christopher W.
Tornabene, Livio L.
TI Origin of small pits in martian impact craters
SO ICARUS
LA English
DT Article
DE Mars, Surface; Cratering; Impact processes; Geological processes;
Terrestrial planets
ID EXPLOSIVE VOLCANIC-ERUPTIONS; HYDROTHERMAL SYSTEMS; PYROCLASTIC FLOWS;
MARS; MELT; RIES; EJECTA; FLUIDIZATION; EMPLACEMENT; DEPOSITS
AB We propose a numerical model for the formation of the closely-spaced pits found in the thin, ejecta-related deposits superposed on the floors, interior terrace blocks, and near-rim ejecta blankets of well-preserved martian impact craters. Our model predicts the explosive degassing of water from this pitted material, which is assumed to originally be water-bearing, impact melt-rich breccia at the time of deposition. This process is analogous to what occurred in the fall-out suevite deposits at the Ries impact structure in Germany. At Ries, impact heating of water-bearing target material resulted in the rapid degassing of its water and other volatiles. The martian environment plays an important role in enhancing the effects of this degassing by increasing the flow-speed of the escaping gas. The high flow-rate of gas through particulate materials, such as suevite, tends to quickly form segregation channels or vent pipes, similar to those found in the Ries deposits. These pipes act as conduits for the efficient high-speed escape of the gas and small clasts that it entrains. Escaping gas and entrained clasts abraded and eroded the conduit walls, flaring them to form pits above a network of pipes. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Boyce, Joseph M.; Wilson, Lionel; Mouginis-Mark, Peter J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Wilson, Lionel] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England.
[Hamilton, Christopher W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tornabene, Livio L.] Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON N6A 5B7, Canada.
RP Boyce, JM (reprint author), Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
EM jboyce@higp.hawaii.edu; l.wilson@lancaster.ac.uk;
christopher.hamilton@nasa.gov; ltornabe@uwo.ca
FU NASA/ASU [A2910]; NASA
FX We thank Drs. Nadine Barlow, Veronica Bray, and an anonymous reviewer
for their thoughtful comments on this work, which was supported under
NASA/ASU THEMIS Team Contract A2910. 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. This is HIGP contribution 1979 and SOEST
contribution 8700.
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 262
EP 275
DI 10.1016/j.icarus.2012.07.027
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200023
ER
PT J
AU Gautier, T
Carrasco, N
Mahjoub, A
Vinatier, S
Giuliani, A
Szopa, C
Anderson, CM
Correia, JJ
Dumas, P
Cernogora, G
AF Gautier, Thomas
Carrasco, Nathalie
Mahjoub, Ahmed
Vinatier, Sandrine
Giuliani, Alexandre
Szopa, Cyril
Anderson, Carrie M.
Correia, Jean-Jacques
Dumas, Paul
Cernogora, Guy
TI Mid- and far-infrared absorption spectroscopy of Titan's aerosols
analogues
SO ICARUS
LA English
DT Article
DE Infrared observations; Prebiotic chemistry; Titan, atmosphere
ID CM(-1) SPECTRAL RANGE; OPTICAL-CONSTANTS; THOLINS; ATMOSPHERE; PLASMA;
CONSTRAINTS; CHEMISTRY; HAZE
AB In this work we present mid- and far-infrared absorption spectra of Titan's aerosol analogues produced in the PAMPRE experimental setup. The evolution of the linear absorption coefficient epsilon (cm(-1)) is given as a function of the wavenumber.
We provide a complete dataset regarding the influence that the concentration of methane vapor in the gas mixture has on the tholin spectra. Among other effects, the intensity of the 2900 cm(-1) (3.4 mu m) pattern (attributed to methyl stretching modes) increases when the methane concentration increases. More generally, tholins produced with low methane concentrations seem to be more amine based polymers, whereas tholins produced with higher methane concentrations contains more aliphatic carbon based structures.
Moreover, it is shown that the position of the bands around 2900 cm(-1) depends on the chemical environment of the methyl functional group. We conclude that the presence of these absorption bands in Titan's atmosphere, as measured with the VIMS instrument onboard Cassini is in agreement with an aerosol contribution.
We also compare the far-infrared spectrum of tholin to spectra of Titan's aerosols derived from recent Cassini-CIRS observations displaying many similarities, particularly with absorption bands at 325 cm(-1), 515 cm(-1), and the methyl attributed 1380 cm(-1) and 1450 cm(-1) bands. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Gautier, Thomas; Carrasco, Nathalie; Mahjoub, Ahmed; Szopa, Cyril; Correia, Jean-Jacques; Cernogora, Guy] Univ Paris 06, UPMC, Univ Versailles St Quentin, CNRS,LATMOS, F-78280 Guyancourt, France.
[Vinatier, Sandrine] Observ Paris, LESIA, F-92195 Meudon, France.
[Giuliani, Alexandre; Dumas, Paul] Synchrotron SOLEIL, F-91192 Gif Sur Yvette, France.
[Giuliani, Alexandre] INRA, CEPIA U1008, F-44316 Nantes, France.
[Anderson, Carrie M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Gautier, T (reprint author), Univ Paris 06, UPMC, Univ Versailles St Quentin, CNRS,LATMOS, 11 Bvd dAlembert, F-78280 Guyancourt, France.
EM thomas.gautier@latmos.ipsl.fr
RI Anderson, Carrie/C-8097-2012; Giuliani, Alexandre/C-1476-2011; szopa,
cyril/C-6865-2015
OI Giuliani, Alexandre/0000-0003-1710-4933; szopa,
cyril/0000-0002-0090-4056
FU CNRS (PNP) [ANR-09-JCJC-0038]; SOLEIL synchrotron facility [20100103]
FX This work was financially supported by CNRS (PNP, ANR-09-JCJC-0038
contract). All the PAMPRE team gratefully thanks the SMIS beam line team
for their help and contribution and SOLEIL synchrotron facility for
accepting and supporting the Project No. 20100103.
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SN 0019-1035
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JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 320
EP 327
DI 10.1016/j.icarus.2012.07.025
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200029
ER
PT J
AU Cloutis, EA
Hudon, P
Hiroi, T
Gaffey, MJ
Mann, P
Bell, JF
AF Cloutis, E. A.
Hudon, P.
Hiroi, T.
Gaffey, M. J.
Mann, P.
Bell, J. F., III
TI Spectral reflectance properties of carbonaceous chondrites: 6. CV
chondrites
SO ICARUS
LA English
DT Article
DE Meteorites; Asteroids; Spectroscopy
ID FE-57 MOSSBAUER-SPECTROSCOPY; X-RAY-DIFFRACTION; ALLENDE METEORITE;
AQUEOUS ALTERATION; PARENT BODY; MINERAL CHEMISTRY; ISOTOPIC
COMPOSITIONS; DARK INCLUSIONS; ORGANIC-MATTER; REFRACTORY INCLUSIONS
AB Multiple reflectance spectra of 11 CV chondrites have been measured to determine spectral-compositional relationships for this meteorite class and to aid the search for CV parent bodies. The reflectance of CV chondrite spectra is variable, ranging from similar to 5% to 13% at 0.56 mu m, and similar to 5% to 15% at the 0.7 mu m region local reflectance maximum. Overall slopes range from slightly blue to red for powders, while slab spectra are strongly blue-sloped. With increasing average grain size and/or removal of the finest fraction, CV spectra generally become more blue-sloped. CV spectra are characterized by ubiquitous absorption features in the 1 and 2 mu m regions. The 1 mu m region is usually characterized by a band centered near 1.05-1.08 mu m and a band or shoulder near 1.3 mu m that are characteristic of Fe-rich olivine. Band depths in the 1 mu m region for powdered CVs and slabs range from similar to 1% to 10%. The 2 mu m region is characterized by a region of broad absorption that extends beyond 2 mu m and usually includes band minima near 1.95 and 2.1 mu m; these features are characteristic of Fe2+-bearing spinel. The sample suite is not comprehensive enough to firmly establish whether spectral differences exist between CVR, CVOxA, and CVOxB subclasses, or as a function of metamorphic grade. However, we believe that the mineralogic and petrologic differences that exist between these classes, and with varying petrologic subtype (CV3.0->3.7), may not be significant enough to result in measurable spectral differences that exceed spectral variations within a subgroup, within an individual meteorite, or as a function of grain size. Terrestrial weathering seems to affect CV spectra most noticeably in the visible region, resulting in more red-sloped spectra for finds as compared to falls. The search for CV parent bodies should focus on the detection of olivine and spinel absorption bands, specifically absorption features near 1.05, 1.3, 1.95, and 2.1 mu m, as these are the most commonly seen spectral features of CV 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, Lyndon B 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.
[Bell, J. F., III] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 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; Jim.Bell@asu.edu
FU NASA Planetary Geology and Geophysics [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. The PSF facility at the University of Winnipeg
was established with generous support from the Canada Foundation for
Innovation, the Manitoba Research Innovations Fund, and the Canadian
Space Agency. This study was supported by an NSERC Discovery grant to
EAC. The authors also wish to thank Julie Ziffer and an anonymous
reviewer for their many helpful comments which helped improve the
quality and readability of this paper.
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PI SAN DIEGO
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SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 328
EP 358
DI 10.1016/j.icarus.2012.07.007
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200030
ER
PT J
AU Keihm, S
Tosi, F
Kamp, L
Capaccioni, F
Gulkis, S
Grassi, D
Hofstadter, M
Filacchione, G
Lee, S
Giuppi, S
Janssen, M
Capria, M
AF Keihm, S.
Tosi, F.
Kamp, L.
Capaccioni, F.
Gulkis, S.
Grassi, D.
Hofstadter, M.
Filacchione, G.
Lee, S.
Giuppi, S.
Janssen, M.
Capria, M.
TI Interpretation of combined infrared, submillimeter, and millimeter
thermal flux data obtained during the Rosetta fly-by of Asteroid (21)
Lutetia
SO ICARUS
LA English
DT Article
DE Asteroids; Surfaces; Regoliths; Infrared observations; Radio
observations; Cratering
ID NEAR-EARTH ASTEROIDS; THERMOPHYSICAL MODEL; RADIOMETRIC METHOD; SURFACE;
TEMPERATURE; PHYSICS; ALBEDO; SPECTROMETER; INSTRUMENT; EMISSION
AB The European Space Agency's Rosetta spacecraft is the first Solar System mission to include instrumentation capable of measuring planetary thermal fluxes at both near-IR (VIRTIS) and submillimeter-millimeter (smm-mm, MIRO) wavelengths. Its primary mission is a 1 year reconnaissance of Comet 67P/Churyumov-Gerasimenko beginning in 2014. During a 2010 close fly-by of Asteroid 21 Lutetia, the VIRTIS and MIRO instruments provided complementary data that have been analyzed to produce a consistent model of Lutetia's surface layer thermal and electrical properties, including a physical model of self-heating. VIRTIS dayside measurements provided highly resolved 1 K accuracy surface temperatures that required a low thermal inertia, I < 30 J/(K m(2) s(0.5)). MIRO smm and mm measurements of polar night thermal fluxes produced constraints on Lutetia's subsurface thermal properties to depths comparable to the seasonal thermal wave, yielding a model of I < 20 J/(K m(2) s(0.5)) in the upper few centimeters, increasing with depth in a manner very similar to that of Earth's Moon. Subsequent MIRO-based model predictions of the dayside surface temperatures reveal negative offsets of similar to 5-30 K from the higher VIRTIS-measurements. By adding surface roughness in the form of 50% fractional coverage of hemispherical mini-craters to the MIRO-based thermal model, sufficient self-heating is produced to largely remove the offsets relative to the VIRTIS measurements and also reproduce the thermal limb brightening features (relative to a smooth surface model) seen by VIRTIS. The Lutetia physical property constraints provided by the VIRTIS and MIRO data sets demonstrate the unique diagnostic capabilities of combined infrared and submillimeter/millimeter thermal flux measurements. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Keihm, S.; Kamp, L.; Gulkis, S.; Hofstadter, M.; Lee, S.; Janssen, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tosi, F.; Capaccioni, F.; Grassi, D.; Filacchione, G.; Giuppi, S.; Capria, M.] Ist Nazl Astrofis INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
RP Keihm, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Stephen.J.Keihm@jpl.nasa.gov
OI capria, maria teresa/0000-0002-9814-9588; Capaccioni,
Fabrizio/0000-0003-1631-4314; Filacchione, Gianrico/0000-0001-9567-0055;
Grassi, Davide/0000-0003-1653-3066; Tosi, Federico/0000-0003-4002-2434
FU Italian Space Agency; ASI-INAF [I/062/08/0, I/026/05/0]; Jet Propulsion
Laboratory, California Institute of Technology, under National
Aeronautics and Space Administration
FX VIRTIS and MIRO are two of the four remote sensing instruments on the
ESA Rosetta spacecraft. VIRTIS was constructed at the Galileo Avionica
Laboratories (Florence, Italy) under the direction of an
Italian-France-Germany consortium. MIRO was constructed at the Jet
Propulsion Laboratory (JPL) under the direction of a US-France-Germany
science-instrument team. This research was conducted at the INAF-IAPS
Institute (Rome, Italy), supported by the Italian Space Agency, ASI-INAF
Grant I/062/08/0, and under ASI-INAF Contract I/026/05/0 and at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. We
thank Michael Mueller and Marco Delbo for their invaluable reviews which
led to important improvements in the manuscript. We also thank the named
individuals in Jorda et al. (2011) and the entire OSIRIS Team for making
their Lutetia shape model available to us prior to publication.
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PI SAN DIEGO
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SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 395
EP 404
DI 10.1016/j.icarus.2012.08.002
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200034
ER
PT J
AU Davies, AG
Veeder, GJ
Matson, DL
Johnson, TV
AF Davies, Ashley Gerard
Veeder, Glenn J.
Matson, Dennis L.
Johnson, Torrence V.
TI Charting thermal emission variability at Pele, Janus Patera and
Kanehekili Fluctus with the Galileo NIMS Io Thermal Emission Database
(NITED)
SO ICARUS
LA English
DT Article
DE Io; Jupiter, Satellites; Volcanism
ID INFRARED MAPPING SPECTROMETER; VOLCANIC ACTIVITY; LAVA LAKES; HOT-SPOTS;
MOON IO; ERUPTION; SSI; TEMPERATURE; SIGNATURE
AB Using the NIMS Io Thermal Emission Database (NITED), a collection of over 1000 measurements of radiant flux from Io's volcanoes (Davies, A.G. et al. [2012]. Geophys. Res. Lett. 39, L01201. doi:10.1029/2011GL049999), we have examined the variability of thermal emission from three of Io's volcanoes: Pele, Janus Patera and Kanehekili Fluctus. At Pele, the 5-mu m thermal emission as derived from 28 night time observations is remarkably steady at 37 +/- 10 GW mu m(-1), re-affirming previous analyses that suggested that Pole an active. rapidly overturning silicate lava lake. Janus Patera also exhibits relatively steady 5-mu m thermal emission (approximate to 20 +/- 3 GW mu m(-1)) in the four observations where Janus is resolved from nearby Kanehekili Fluctus. Janus Patera might contain a Pele-like lava lake with an effusion rate (Q(F)) of approximate to 40-70 m(3) s(-1). It should be a prime target for a future mission to Io in order to obtain data to determine lava eruption temperature. Kanehekili Fluctus has a thermal emission spectrum that is indicative of the emplacement of lava flows with insulated crusts. Effusion rate at Kanehekili Fluctus dropped by an order of magnitude from approximate to 95 m(3) s(-1) in mid-1997 to approximate to 4 m(3) s(-1) in late 2001. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Davies, Ashley Gerard; Matson, Dennis L.; Johnson, Torrence V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Veeder, Glenn J.] Bear Fight Inst, Winthrop, WA 98862 USA.
RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-401, Pasadena, CA 91109 USA.
EM Ashley.Davies@jpl.nasa.gov
FU NASA
FX This work was conducted at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA, and is supported by
the NASA Outer Planets Research Program. We thank Oleg Abramov and David
Williams for their reviews. (C) 2012 Caltech. All rights reserved.
NR 32
TC 8
Z9 8
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2012
VL 221
IS 1
BP 466
EP 470
DI 10.1016/j.icarus.2012.04.012
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017VV
UT WOS:000309620200041
ER
PT J
AU Cantrell, JH
Yost, WT
AF Cantrell, John H.
Yost, William T.
TI Energy conservation and pulse propagation in an elastic medium with
quadratic nonlinearity
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID AMPLITUDE ULTRASONIC WAVES; ACOUSTIC-RADIATION STRESS; FUSED-SILICA;
SOLIDS; 3-DEGREES-K; PARAMETERS; CONSTANTS; ALUMINUM; COPPER
AB A sinusoidal acoustic tone-burst launched into an elastic medium with weak quadratic nonlinearity is shown to generate a right-triangular static displacement pulse, when conservation of energy is properly imposed on the model equations. The right-triangular displacement profile is shown to occur whether the tone-burst is modeled with displacement-prescribed or traction-prescribed boundary conditions. Definitive experimental evidence is presented confirming the model predictions. Theoretical arguments and experimental evidence are also presented showing that, contrary to the assertion of Qu et al. [J. Acoust. Soc. Am. 131, 1827 (2012)], the right-triangular shape is not in violation of causality. [http://dx.doi.org/10.1063/1.4748963]
C1 [Cantrell, John H.; Yost, William T.] NASA, Langley Res Ctr, Res Directorate, Hampton, VA 23681 USA.
RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Res Directorate, Hampton, VA 23681 USA.
EM john.h.cantrell@nasa.gov; William.t.yost@nasa.gov
NR 21
TC 1
Z9 1
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD SEP 1
PY 2012
VL 112
IS 5
AR 053507
DI 10.1063/1.4748963
PG 6
WC Physics, Applied
SC Physics
GA 010CN
UT WOS:000309072200038
ER
PT J
AU Applebaum, M
Eppard, M
Hall, L
Blevins, J
AF Applebaum, Michael
Eppard, Marc
Hall, Les
Blevins, John
TI Protuberance Aerodynamic Loads for Space Launch Vehicle Systems Using
Computational Fluid Dynamics
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 29th AIAA Applied Aerodynamics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA
AB This paper present's the methodology used to determine the protuberance aerodynamic loads for NASA's Ares I Crew Launch Vehicle. The methodology presented used computational fluid dynamics to obtain pressures and forces on the protuberances. This is one of the first times computational fluid dynamics has been used to estimate protuberance aerodynamic loads for such a complicated configuration. The approach used a discrete matrix of computational fluid dynamics simulations and decomposed the protuberance in a manner suitable to give both the structural and venting engineers useful data. One of the guiding principles in the development of the data book was that the data book was to be used for analysis of protuberances and not in the design of the protuberance. In this regard, the data book contained significant conservatism both in the methodology and in the choice for a factor of conservatism. The methodology, along with advantages and disadvantages to the current approach, is discussed. Two examples of protuberances in the Ares I Aerodynamic Data Book are given.
C1 [Applebaum, Michael; Eppard, Marc; Hall, Les] CRM Solut Inc, Huntsville, AL 35802 USA.
[Blevins, John] NASA, George C Marshall Space Flight Ctr, Aerodynam Team, Aerosci Branch,EV33, Huntsville, AL 35802 USA.
RP Applebaum, M (reprint author), CRM Solut Inc, Huntsville, AL 35802 USA.
NR 9
TC 0
Z9 0
U1 0
U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 779
EP 787
DI 10.2514/1.A32171
PG 9
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800003
ER
PT J
AU Sekula, MK
Piatak, DJ
Rausch, RD
AF Sekula, Martin K.
Piatak, David J.
Rausch, Russ D.
TI Analysis of Ares Crew Launch Vehicle Transonic Alternating Flow
Phenomenon
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 28th AIAA Applied Aerodynamics Conference
CY JUN 28-JUL 01, 2010
CL Chicago, IL
SP AIAA
AB A wind-tunnel test of the Ares I-X rigid buffet model identified unusually large buffet loads. These loads were produced by an alternating flow phenomenon at the crew-module/service-module junction. The conical design of the Ares I-X crew module and the cylindrical design of the service module expose the vehicle to unsteady pressure loads due to the sudden transition between a subsonic separated and a supersonic attached flow about the cone cylinder junction as the local flow randomly fluctuates back and forth between the two flow states. These fluctuations produce a square-wave-like pattern in the pressure time histories, resulting in large-amplitude impulsive buffet loads. Subsequent testing of the Ares I rigid buffet model found lower buffet loads because the evolved Ares I design includes an ogive fairing that covers the crew-module/service-module junction, thereby making the vehicle less susceptible to the onset of alternating flow. An analysis of the phenomenon indicates that it is most severe at low angles of attack and exacerbated by the presence of vehicle protuberances. A comparison of impulsive loads derived from wind-tunnel and flight-test data for the Ares I-X indicates significant overpredictions in magnitude and duration of the buffet load.
C1 [Sekula, Martin K.; Piatak, David J.; Rausch, Russ D.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
RP Sekula, MK (reprint author), NASA, Langley Res Ctr, Aeroelast Branch, Mail Stop 340, Hampton, VA 23681 USA.
NR 9
TC 0
Z9 0
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 788
EP 797
DI 10.2514/1.A32154
PG 10
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800004
ER
PT J
AU Piatak, DJ
Sekula, MK
Rausch, RD
AF Piatak, David J.
Sekula, Martin K.
Rausch, Russ D.
TI Ares Launch Vehicle Transonic Buffet Testing and Analysis Techniques
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 28th AIAA Applied Aerodynamics Conference
CY JUN 28-JUL 01, 2010
CL Chicago, IL
SP AIAA
AB It is necessary to define the launch vehicle buffet loads to ensure that launch vehicle structural components and subsystems possess adequate strength, stress, and fatigue margins when the vehicle structural dynamic response to these buffet loads is considered. A buffet wind-tunnel test program was developed for the Ares Crew Launch Vehicle and employed 3.5% scale rigid models of the Ares I and Ares I-X launch vehicles. These models were tested at transonic conditions at the Transonic Dynamics Tunnel at NASA Langley Research Center and each was instrumented with 256 unsteady pressure transducers to measure the buffet environment across the desired frequency range. The deliverable of the Ares buffet test program was full-scale buffet forcing functions derived from integrating the measured fluctuating pressures on these rigid wind-tunnel models. These buffet forcing functions were then used as input to a multimode structural analysis to determine the vehicle response to buffet and the resulting buffet loads and accelerations. This paper discusses the development of the Ares I and I-X rigid buffet model test programs from the standpoint of model design, instrumentation system design, test implementation, and data analysis techniques to yield final products, and then presents normalized sectional buffet forcing function root-mean-squared levels.
C1 [Piatak, David J.; Sekula, Martin K.; Rausch, Russ D.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
RP Piatak, DJ (reprint author), NASA, Langley Res Ctr, Aeroelast Branch, Mail Stop 340, Hampton, VA 23681 USA.
NR 13
TC 1
Z9 1
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 798
EP 807
DI 10.2514/1.A32175
PG 10
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800005
ER
PT J
AU Hanke, JL
AF Hanke, Jeremy L.
TI Detailed Uncertainty Analysis of the Ares I A106 Liftoff/Transition
Database
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 29th AIAA Applied Aerodynamics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA
AB The Ares I A106 Liftoff/Transition Force and Moment Aerodynamics Database modeled the aerodynamics of the Ares I crew launch vehicle from the moment of liftoff through the transition from high to low total angles of attack and included the effects of the launch tower on the vehicle aerodynamics. The database was developed from wind-tunnel data acquired in NASA Langley Research Center's 14- by 22-Foot Subsonic Wind Tunnel using a 1.75% scale model of the vehicle and tower assembly. The uncertainty model contained contributions from three primary sources: experimental uncertainty, database modeling uncertainty, and database query interpolation uncertainty. The uncertainty for each source was quantified using the available data, and the total uncertainty was a root-sum-square combination of the three sources. The most significant uncertainty source was experimental uncertainty. The database and uncertainty model yielded significant improvements in the fidelity of the aerodynamic predictions for this flight regime over previous estimates based on limited computational and empirical data for the Ares I-X flight test vehicle. In addition, the maximum aerodynamic force in a dispersed case pushing the vehicle toward the launch tower assembly was 40% lower than the worst-case estimate from the previous data.
C1 NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Hanke, JL (reprint author), NASA, Langley Res Ctr, Configurat Aerodynam Branch, Mail Stop 499, Hampton, VA 23681 USA.
NR 20
TC 0
Z9 0
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 808
EP 821
DI 10.2514/1.A32291
PG 14
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800006
ER
PT J
AU Piatak, DJ
Sekula, MK
Rausch, RD
AF Piatak, David J.
Sekula, Martin K.
Rausch, Russ D.
TI Comparison of Ares I-X Wind-Tunnel-Derived Buffet Environment with
Flight Data
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 29th AIAA Applied Aerodynamics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA
AB The Ares I-X flight-test vehicle, launched in October 2009, carried with it 243 buffet-verification pressure sensors and was one of the most heavily instrumented launch-vehicle flight tests ever conducted. This flight test represented a unique opportunity for NASA and its partners to compare the wind-tunnel-derived buffet environment with that measured during the flight of Ares I-X. This paper discusses the comparison of these wind-tunnel-derived and flight-test-measured buffet environments, including fluctuating pressure coefficient and normalized sectional buffet-forcing-function root-mean-square magnitudes, frequency content of power-spectral-density functions, and force magnitudes of an alternating flow phenomena. Comparison of wind-tunnel-model and flight-test-vehicle buffet environments showed very good agreement with root-mean-square magnitudes of buffet-forcing functions at the majority of vehicle stations. Spectra proved a challenge to compare because of different wind-tunnel and flight-test conditions and data acquisition rates; however, meaningful and promising comparisons of buffet spectra are presented. Lastly, the buffet loads resulting from the transition of subsonic separated flow to supersonic attached flow were significantly overpredicted by wind-tunnel results.
C1 [Piatak, David J.; Sekula, Martin K.; Rausch, Russ D.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
RP Piatak, DJ (reprint author), NASA, Langley Res Ctr, Aeroelast Branch, Mail Stop 340, Hampton, VA 23681 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 822
EP 833
DI 10.2514/1.A32176
PG 12
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800007
ER
PT J
AU Pinier, JT
AF Pinier, Jeremy T.
TI New Aerodynamic Data Dispersion Method with Application to Launch
Vehicle Design
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 29th AIAA Applied Aerodynamics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA
AB This paper describes a new generalized method for implementing aerodynamic data dispersions in the framework of Monte Carlo flight simulations. As opposed to the traditional pure-bias type dispersion methods, the new proposed model is a general mathematical approach based on truncated Fourier series that, when combined with physical modeling tailored to the aerodynamic quantity of interest, enables the generation of more realistically dispersed data with magnitude, phase, slope variations, and a controlled amount of bias. The new method is also presented in a particular example, as applied to the Ares I-X Flight-Test Vehicle and the Ares I Crew Launch Vehicle rolling moment data. It is shown how the adoption and implementation of this new method within these projects has resulted in significant increases in predicted roll control authority and has lowered the induced risks for Night-test operations. A direct impact on launch vehicles is a reduced size for auxiliary control systems and the possibility of an increased payload. This technique has the potential of being applied to problems in multiple areas where nominal data together with uncertainties are used to produce simulations using Monte Carlo type random sampling methods. It is shown that physics-based dispersion models, together with nominal data and uncertainties, can make flight simulations more realistic and allow for leaner spacecraft designs.
C1 NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Pinier, JT (reprint author), NASA, Langley Res Ctr, Configurat Aerodynam Branch, MS 499, Hampton, VA 23681 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 834
EP 841
DI 10.2514/1.A32219
PG 8
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800008
ER
PT J
AU Pinier, JT
AF Pinier, Jeremy T.
TI Ares I and Ares I-X Stage Separation Aerodynamic Testing
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 49th AIAA Aerospace Sciences Meeting including the New Horizons Forum
and Aerospace Exposition
CY JAN 03-07, 2011
CL Orlando, FL
SP AIAA
AB The aerodynamics of the Ares I Crew Launch Vehicle and Ares I-X Flight-Test Vehicle during stage separation was characterized by testing 1%-scale models at the Arnold Engineering Development Center's Von Karman Gas Dynamics Facility Tunnel A at Mach numbers of 4.5 and 5.5. To fill a large matrix of data points in an efficient manner, an injection system supported the upper stage and a captive trajectory system was used as a support system for the first stage located downstream of the upper stage. In an overall very successful and productive test, this complex experimental setup, in conjunction with advanced postprocessing of the wind-tunnel data, has enabled the construction of a multidimensional aerodynamic database for the analysis and simulation of the critical phase of stage separation at high supersonic Mach numbers. Historical data are not readily available for comparison on this type of vehicle and Reynolds-averaged Navier Stokes computational solutions remain far from being a reliable source of static aerodynamic data for this complex flowfield. Therefore, an extensive set of data from repeated wind-tunnel runs was purposefully obtained to ensure that the experimental uncertainty would be accurately quantified.
C1 NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Pinier, JT (reprint author), NASA, Langley Res Ctr, Configurat Aerodynam Branch, MS 499, Hampton, VA 23681 USA.
NR 13
TC 0
Z9 0
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 842
EP 852
DI 10.2514/1.A32220
PG 11
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800009
ER
PT J
AU Pinier, JT
Hanke, JL
Tomek, WG
AF Pinier, Jeremy T.
Hanke, Jeremy L.
Tomek, William G.
TI Ares I Aerodynamic Testing at the Boeing Polysonic Wind Tunnel
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 49th AIAA Aerospace Sciences Meeting including the New Horizons Forum
and Aerospace Exposition
CY JAN 03-07, 2011
CL Orlando, FL
SP AIAA
AB Throughout three full design analysis cycles, the Ares I Project within the Constellation Program has consistently relied on the Boeing Polysonic Wind Tunnel for aerodynamic testing of the subsonic, transonic, and supersonic portions of the atmospheric flight envelope (Mach = 0.5 to 4.5). Each full design cycle required the development of aerodynamic databases for the six-degree-of-freedom forces and moments, as well as distributed line loads databases covering the full range of Mach number, total angle of attack, and aerodynamic roll angle. The high-fidelity data collected in this facility have been consistent with the data collected in NASA Langley's Unitary Plan Wind Tunnel at the overlapping condition of Mach = 1.6. Much insight into the aerodynamic behavior of the launch vehicle during all phases of flight was gained through wind-tunnel testing. Important knowledge pertaining to slender launch vehicle aerodynamics in particular was accumulated, including the rolling moment mitigation effect of aerodynamic strakes, when placed judiciously, as well as the impacts of shock reflection on these types of vehicles at transonic conditions. In conducting these wind-tunnel tests and developing experimental aerodynamic databases, some challenges with model scale, pressure measurement lags, and temperature gradients were encountered. These are reported as lessons learned in this paper for the benefit of future launch vehicle aerodynamic developments.
C1 [Pinier, Jeremy T.; Hanke, Jeremy L.; Tomek, William G.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Pinier, JT (reprint author), NASA, Langley Res Ctr, Configurat Aerodynam Branch, MS 499, Hampton, VA 23681 USA.
NR 7
TC 3
Z9 4
U1 0
U2 4
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 853
EP 863
DI 10.2514/1.A32221
PG 11
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800010
ER
PT J
AU Pamadi, BN
Pei, J
Pinier, JT
Holland, SD
Covell, PF
Klopfer, GH
AF Pamadi, Bandu N.
Pei, Jing
Pinier, Jeremy T.
Holland, Scott D.
Covell, Peter F.
Klopfer, Goetz H.
TI Aerodynamic Analyses and Database Development for Ares I Vehicle
First-Stage Separation
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 49th AIAA Aerospace Sciences Meeting including the New Horizons Forum
and Aerospace Exposition
CY JAN 03-07, 2011
CL Orlando, FL
SP AIAA
AB This paper presents the aerodynamic analysis and database development for the first-stage separation of the Ares! A106 Crew Launch Vehicle configuration. Separate databases were created for the first stage and upper stage. Each database consists of three components: isolated or freestream coefficients, power-off proximity increments, and power-on proximity increments. The power-on database consists of three parts, all plumes firing at nominal conditions, the one booster deceleration motor out condition, and the one ullage settling motor out condition. The isolated and power-off incremental databases were developed using wind-tunnel test data. The power-on proximity increments were developed using computational fluid dynamics solutions.
C1 [Pamadi, Bandu N.; Holland, Scott D.; Covell, Peter F.] NASA, Langley Res Ctr, Langley Ares Project Off, Hampton, VA 23681 USA.
[Pamadi, Bandu N.; Pei, Jing; Covell, Peter F.] NASA, Langley Res Ctr, Vehicle Anal Branch, Syst Anal & Concepts Directorate, Hampton, VA 23681 USA.
[Pinier, Jeremy T.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
[Holland, Scott D.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Klopfer, Goetz H.] NASA, Ames Res Ctr, Modeling & Simulat Applicat Branch, Adv Supercomp Div,Explorat Syst Mission Directora, Moffett Field, CA 94035 USA.
RP Pamadi, BN (reprint author), NASA, Langley Res Ctr, Langley Ares Project Off, Hampton, VA 23681 USA.
EM Bandu.N.Pamadi@nasa.gov; Jing.Pei-1@nasa.gov; T.Pinier@nasa.gov;
Scott.D.Holland@nasa.gov; Peter.F.Covell@nasa.gov;
Goetz.H.Klopfer@nasa.gov
NR 10
TC 2
Z9 4
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 864
EP 874
DI 10.2514/1.A32247
PG 11
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800011
ER
PT J
AU White, S
AF White, S.
TI Solar Tower Radiation Testing of Phenolic Impregnated Carbon Ablator
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 10th AIAA/ASME Joint Thermophysics and Heat Transfer Conference
CY JUN 28-JUL 01, 2010
CL Chicago, IL
SP AIAA, ASME
AB Sandia National Laboratory's National Solar Tower Thermal Test Facility was used to irradiate specimens of Phenolic Impregnated Carbon Ablator to evaluate whether or not this thermal protection material would exhibit in-depth transmission and absorption, and therefore would respond differently to potential shock-layer radiative heating than to convective heating. Tests were run at 50, 100, and 150 W/cm(2) levels of concentrated solar radiation. Experimental results are presented both from spectral measurements on thin radiation transport test specimens, as well as from in-depth temperature measurements. Both spectral measurements and measured in-depth temperature profiles showed that, although it is a porous low-density material, this material did not exhibit problematic transmission or in-depth absorption at the tested high levels of near-infrared radiation, for all pragmatic centimeter-to-inch scale thicknesses. This low-density carbon-fiber-based ablator functioned as a surface absorber to efficiently absorb the incident visible and near infrared incident radiation in the top 2 mm layer at radiative flux levels up to 150 W/cm(2).
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP White, S (reprint author), NASA, Ames Res Ctr, Mail Stop 234-1, Moffett Field, CA 94035 USA.
NR 14
TC 0
Z9 0
U1 1
U2 5
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 889
EP 893
DI 10.2514/1.A32104
PG 5
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800013
ER
PT J
AU Milos, FS
Chen, YK
Gokcen, T
AF Milos, F. S.
Chen, Y-K
Goekcen, T.
TI Nonequilibrium Ablation of Phenolic Impregnated Carbon Ablator
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 48th AIAA Aerospace Sciences Meeting and Exhibit / New Horizons Forum
and Aerospace Exposition
CY JAN 04-08, 2010
CL Orlando, FL
SP AIAA
AB In previous work, an equilibrium ablation and thermal response model for Phenolic Impregnated Carbon Ablator was developed. In general, over a wide range of test conditions, model predictions compared well with arcjet data for surface recession, surface temperature, in-depth temperature at multiple thermocouples, and char depth. In this work, additional arcjet tests were conducted at stagnation conditions down to 40 W/cm(2) and 1.61 kPa. The new data suggest that nonequilibrium effects become important for ablation predictions at heat flux or pressure below about 80 W/cm(2) or 10 kPa, respectively. Modifications to the ablation model to account for nonequilibrium effects are investigated. Predictions of the equilibrium and nonequilibrium models are compared with the arcjet data.
C1 [Milos, F. S.; Chen, Y-K] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Goekcen, T.] ELORET Corp, Sunnyvale, CA 94086 USA.
RP Milos, FS (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, Mail Stop 234-1, Moffett Field, CA 94035 USA.
NR 16
TC 4
Z9 4
U1 2
U2 10
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 894
EP 904
DI 10.2514/1.A32298
PG 11
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800014
ER
PT J
AU Coleman, MJ
Baginski, F
Romanofsky, RR
AF Coleman, Michael J.
Baginski, Frank
Romanofsky, Robert R.
TI Effect of Boundary Support and Reflector Dimensions on Inflatable
Parabolic Antenna Performance
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 51st AIAA/ASME/ASCE/AHS/ASC Structures, Structural Dynamics, and
Materials Conference / 11th AIAA Gossamer Systems Forum
CY APR 10-15, 2010
CL Orlando, FL
SP AIAA, AHS, ASME, ASC, ASCE, US Off Naval Res (ONR), US AF Off Sci Res (AFOSR)
ID DEFORMATIONS; MEMBRANES
AB For parabolic antennas with sufficient surface accuracy, more power can be radiated with a larger aperture size. This paper explores the performance of antennas of various size and reflector depth. The particular focus is on a large inflatable elastic antenna reflector that is supported about its perimeter by a set of elastic tendons and is subjected to a constant hydrostatic pressure. The surface accuracy of the antenna is measured by an rms calculation, whereas the reflector phase error component of the efficiency is determined by computing the power density at boresight. In the analysis, the calculation of antenna efficiency is not based on the Ruze Equation. Hence, no assumption regarding the distribution of the reflector surface distortions is presumed. The reflector surface is modeled as an isotropic elastic membrane using a linear stress strain constitutive relation. Three types of antenna reflector construction are considered: one molded to an ideal parabolic form and two different flat panel design patterns. The flat panel surfaces are constructed by seaming together panels in a manner that the desired parabolic shape is approximately attained after pressurization. Numerical solutions of the model problem are calculated under a variety of conditions to estimate the accuracy and efficiency of these antenna systems. In the case of the flat panel constructions, several different cutting patterns are analyzed to determine an optimal cutting strategy.
C1 [Coleman, Michael J.; Baginski, Frank] George Washington Univ, Dept Math, Washington, DC 20052 USA.
[Romanofsky, Robert R.] NASA, John H Glenn Res Ctr Lewis Field, Antenna Microwave & Opt Syst Branch, Cleveland, OH 44135 USA.
RP Coleman, MJ (reprint author), George Washington Univ, Dept Math, Washington, DC 20052 USA.
EM mikec8254@gmail.com; baginski@gwu.edu; robert.r.romanofsky@nasa.gov
NR 20
TC 4
Z9 4
U1 0
U2 7
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 905
EP 914
DI 10.2514/1.A32021
PG 10
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800015
ER
PT J
AU Jegley, DC
Wu, KC
Phelps, JE
McKenney, MJ
Oremont, L
AF Jegley, Dawn C.
Wu, K. Chauncey
Phelps, James E.
McKenney, Martin J.
Oremont, Leonard
TI Structural Efficiency of Composite Struts for Aerospace Applications
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 52nd AIAA/ASME/ASCE/AHS/ASC Structures, Structural Dynamics and
Materials Conference / 19th AIAA/ASME/AHS Adaptive Structures Conference
CY APR 04-07, 2011
CL Denver, CO
SP AIAA, ASME, ASCE, AHS, ASC
ID COMPRESSION
AB The structural efficiency of carbon-epoxy tapered struts is evaluated through trade studies, detailed analysis, manufacturing, and experimentation. Because some of the Altair lunar lander struts are more highly loaded than struts used in applications such as satellites and telescopes, the primary focus of the effort is on these highly loaded struts. Lunar lander requirements include that the strut has to be tapered on both ends, complicating the design and limiting the manufacturing process. Optimal ply stacking sequences, geometries, and materials are determined and the sensitivity of the strut weight to each parameter is evaluated. The trade study results indicate that the most efficient carbon-epoxy struts are 30% lighter than the most efficient aluminum-lithium struts. Structurally efficient, highly loaded struts were fabricated and loaded in tension and compression to determine if they met the design requirements and to verify the accuracy of the analyses. Experimental evaluation of some of these struts demonstrated that they could meet the greatest Altair loading requirements in both tension and compression. These results could be applied to other mass-constrained vehicles requiring struts with high loading.
C1 [Jegley, Dawn C.; Wu, K. Chauncey] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
[Phelps, James E.; McKenney, Martin J.] ATK Space Syst Inc, Struct Dynam Branch, Hampton, VA 23681 USA.
[Oremont, Leonard] Lockheed Martin Corp, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Jegley, DC (reprint author), NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Mail Stop 190, Hampton, VA 23681 USA.
NR 17
TC 1
Z9 3
U1 0
U2 6
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 915
EP 924
DI 10.2514/1.A32085
PG 10
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800016
ER
PT J
AU Hanson, JM
Hill, AD
Beard, BB
AF Hanson, John M.
Hill, Ashley D.
Beard, Bernard B.
TI Launch Vehicle Abort Analysis of Failures Leading to Loss of Control
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/GNandC Conference
CY AUG 08-11, 2011
CL Portland, OR
SP AIAA, GN&C
AB Launch vehicle ascent is a time of high risk for an onboard crew. There is a large fraction of possible failures for which time is of the essence and a successful abort is possible if the detection and action happens quickly enough. This paper focuses on abort determination based on data already available from the guidance, navigation, and control systems. This work is the result of failure analysis efforts performed during the Arcs I launch vehicle development program. The two primary areas of focus are the derivation of abort triggers to ensure that abort occurs as quickly as possible when needed while avoiding false aborts and the evaluation of success in aborting off the failing launch vehicle.
C1 [Hanson, John M.] NASA, George C Marshall Space Flight Ctr, Flight Mech & Anal Div, Huntsville, AL 35812 USA.
[Hill, Ashley D.] Dynamic Concepts Inc, Huntsville, AL 35806 USA.
[Beard, Bernard B.] ARES Corp, Tennessee Valley Off, Huntsville, AL 35805 USA.
EM john.m.hanson@nasa.gov; ahill@dynamic-concepts.com
NR 11
TC 1
Z9 1
U1 0
U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 925
EP 934
DI 10.2514/1.A32061
PG 10
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800017
ER
PT J
AU Bilimoria, KD
Mueller, ER
AF Bilimoria, Karl D.
Mueller, Eric R.
TI Handling Qualities of a Capsule Spacecraft During Atmospheric Entry
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation and Control Conference
CY AUG 02-06, 2010
CL Toronto, CANADA
SP Amer Inst Aeronaut & Astronaut (AIAA)
ID CONTROL POWER; DOCKING; SYSTEM
AB A piloted simulation was conducted to study handling qualities for capsule spacecraft entering the Earth's atmosphere. Eight evaluation pilots, including six pilot astronauts, provided Cooper-Harper ratings, workload ratings, and qualitative comments. The simulation began after descending through the atmospheric entry interface point and continued until the drogue parachutes deployed. There were two categories of piloting tasks, both of which required bank-angle control. In one task category the pilot followed a closed-loop bank-angle guidance command computed by the backup entry guidance system to manage g-loads during entry. In the other task category the pilot used intuitive rules to determine the desired bank angle independently based on an open-loop guidance schedule of vertical speed, Mach, and total energy specified at several range-to-target gates along the entry trajectory. Pilots were able to accurately track the bank-angle guidance commands and steered the capsule toward the recovery site with essentially the same range error as the benchmark autopilot trajectory albeit with substantially higher propellant usage, and the handling qualities for this task were satisfactory. Another key result was that the complex piloting task of atmospheric entry could be performed satisfactorily, even in the presence of large dispersions, by controlling bank angle to follow a simple open-loop guidance schedule.
C1 [Bilimoria, Karl D.; Mueller, Eric R.] NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Moffett Field, CA 94035 USA.
RP Bilimoria, KD (reprint author), NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA.
EM Karl.Bilimoria@nasa.gov; Eric.Mueller@nasa.gov
NR 30
TC 1
Z9 1
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2012
VL 49
IS 5
BP 935
EP 943
DI 10.2514/1.A32101
PG 9
WC Engineering, Aerospace
SC Engineering
GA 017EB
UT WOS:000309571800018
ER
PT J
AU Cunningham, LC
Page, FZ
Simonson, BM
Kozdon, R
Valley, JW
AF Cunningham, Lauren C.
Page, F. Zeb
Simonson, Bruce M.
Kozdon, Reinhard
Valley, John W.
TI Ion microprobe analyses of delta O-18 in early quartz cements from 1.9
Ga granular iron formations (GIFs): A pilot study
SO PRECAMBRIAN RESEARCH
LA English
DT Article
DE Oxygen isotopes; Gunflint Iron Formation; Sokoman Iron Formation;
Cathodoluminescence; Ion microprobe; Quartz diagenesis
ID OXYGEN ISOTOPIC COMPOSITION; PORE FLUID CONSTRAINTS; LABRADOR-TROUGH;
SOUTH-AFRICA; CHERTS; GEOCHEMISTRY; TEMPERATURE; OCEAN; METAMORPHISM;
PETROLOGY
AB The low delta O-18 values of Precambrian cherts have been widely used to infer that temperatures were higher and/or seawater delta O-18 was lower compared to today's oceans. However, the Precambrian cherts presented as evidence for these temperatures are neomorphosed from amorphous precursors that originally precipitated from ocean water, suggesting diagenetic alteration is an important cause of the widespread low-delta O-18 values. Many pores between sand-size clasts in granular iron formations (GIFs) are filled with coarsely crystalline quartz cements that are texturally primary. In unmetamorphosed GIF samples from the 1.9 Ga Gunflint and Sokoman iron formations, synsedimentary clasts of GIF and high minus-cement porosities (the volume of pore space occupied by recognizable cement, inversely proportional to the degree of compaction) indicate such cements precipitated directly from pore water near the depositional interface. Growth bands identified in quartz cement crystals using cathodoluminescence (CL) imaging further confirm their void-filling and unrecrystallized nature. In order to test the effect of neomorphism on the delta O-18 of silica in these rocks, unrecrystallized primary quartz cements and neomorphic quartz in adjacent clasts were both analyzed by ion microprobe. Values of delta O-18 range from 23.5 to 26.4 parts per thousand. VSMOW in cements and 21.3-26.8 parts per thousand in clasts in samples from the Gunflint Iron Formation. Samples from the Sokomon Iron Formation record deeper, more evolved pore waters and in some cases contain lower delta O-18 cements. In individual pores of Gunflint samples, cement values vary only slightly more than analytical uncertainty from edge to center and no consistent increasing or decreasing trends were observed. Overall, the delta O-18 of the cements are similar to the most elevated delta O-18 reported from cherts of similar age, but span a substantially smaller range. This suggests most of the lower values reported previously reflect late-diagenetic conditions at greater burial depths. The shallow, possibly restricted seas above the Gunflint and Sokoman GIFs appear to have been warmer and may have been lower in delta O-18 than present-day seawater, but they may not have been representative of global seawater. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Cunningham, Lauren C.; Page, F. Zeb; Simonson, Bruce M.] Oberlin Coll, Dept Geol, Oberlin, OH 44074 USA.
[Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, Dept Geosci, WiscSIMS, NASA,Astrobiol Inst, Madison, WI 53706 USA.
RP Simonson, BM (reprint author), Oberlin Coll, Dept Geol, 52 W Lorain St, Oberlin, OH 44074 USA.
EM bruce.simonson@oberlin.edu
RI Page, F. Zeb/N-4563-2014; Kozdon, Reinhard/J-9468-2014; Valley,
John/B-3466-2011
OI Page, F. Zeb/0000-0002-2100-0806; Kozdon, Reinhard/0000-0001-6347-456X;
Valley, John/0000-0003-3530-2722
FU Oberlin College; NASA [NNX08AI29G]; NASA Astrobiology Institute; DOE
[93ER14389]; NSF-CCLI [0087895]; NSF-EAR [0319230, 0744079, 1053466]
FX Petrographic research was supported by grants from Oberlin College and
NASA (NNX08AI29G). Thanks are extended to Eric Essene and Carl Henderson
at the University of Michigan for access to and assistance with the
electron probe microanalyzer used to obtain CL images. We also thank
Hubert Bates and Peter Munk for preparing the thin sections, Noriko Kita
for assistance with ion microprobe analysis, and Andrey Bekker and 2
anonymous reviewers for valuable feedback on our initial draft.
Geochemical research was partly supported by the NASA Astrobiology
Institute, DOE (93ER14389), and Oberlin College. The acquisition of the
SEM at Oberlin College used in this study was supported by NSF-CCLI
(0087895). WiscSIMS is partly supported by NSF-EAR (0319230, 0744079,
1053466).
NR 59
TC 1
Z9 1
U1 1
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0301-9268
J9 PRECAMBRIAN RES
JI Precambrian Res.
PD SEP
PY 2012
VL 214
SI SI
BP 258
EP 268
DI 10.1016/j.precamres.2012.01.016
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA 014KC
UT WOS:000309373500016
ER
PT J
AU Hoare, MG
Purcell, CR
Churchwell, EB
Diamond, P
Cotton, WD
Chandler, CJ
Smethurst, S
Kurtz, SE
Mundy, LG
Dougherty, SM
Fender, RP
Fuller, GA
Jackson, JM
Garrington, ST
Gledhill, TR
Goldsmith, PF
Lumsden, SL
Marti, J
Moore, TJT
Muxlow, TWB
Oudmaijer, RD
Pandian, JD
Paredes, JM
Shepherd, DS
Spencer, RE
Thompson, MA
Umana, G
Urquhart, JS
Zijlstra, AA
AF Hoare, M. G.
Purcell, C. R.
Churchwell, E. B.
Diamond, P.
Cotton, W. D.
Chandler, C. J.
Smethurst, S.
Kurtz, S. E.
Mundy, L. G.
Dougherty, S. M.
Fender, R. P.
Fuller, G. A.
Jackson, J. M.
Garrington, S. T.
Gledhill, T. R.
Goldsmith, P. F.
Lumsden, S. L.
Marti, J.
Moore, T. J. T.
Muxlow, T. W. B.
Oudmaijer, R. D.
Pandian, J. D.
Paredes, J. M.
Shepherd, D. S.
Spencer, R. E.
Thompson, M. A.
Umana, G.
Urquhart, J. S.
Zijlstra, A. A.
TI The Coordinated Radio and Infrared Survey for High-Mass Star Formation
(The CORNISH Survey). I. Survey Design
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID GALACTIC PLANE SURVEY; H-II REGIONS; YOUNG STELLAR OBJECTS; KINEMATIC
DISTANCE AMBIGUITY; ULTRACOMPACT HII-REGIONS; X-RAY BINARIES; VLA SKY
SURVEY; O-TYPE STARS; MOLECULAR CLOUDS; SOURCE CATALOG
AB We describe the motivation, design, and implementation of the CORNISH survey, an arcsecond-resolution radio continuum survey of the inner galactic plane at 5 GHz using the Very Large Array (VLA). It is a blind survey coordinated with the northern Spitzer GLIMPSE I region covering 10 degrees < l < 65 degrees and vertical bar b vertical bar < 1 degrees at similar resolution. We discuss in detail the strategy that we employed to control the shape of the synthesised beam across this survey, which covers a wide range of fairly low declinations. Two snapshots separated by 4(h) kept the beam elongation to less that 1.5 over 75% of the survey area and less than 2 over 98% of the survey. The prime scientific motivation is to provide an unbiased survey for ultra-compact H II regions to study this key phase in massive star formation. A sensitivity around 2 mJy will allow the automatic distinction between radio-loud and radio-quiet mid-IR sources found in the Spitzer surveys. This survey has many legacy applications beyond star formation, including evolved stars, active stars and binaries, and extragalactic sources. The CORNISH survey for compact ionized sources complements other Galactic plane surveys that target diffuse and nonthermal sources, as well as atomic and molecular phases to build up a complete picture of the interstellar medium in the Galaxy.
C1 [Hoare, M. G.; Purcell, C. R.; Lumsden, S. L.; Oudmaijer, R. D.; Urquhart, J. S.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Purcell, C. R.; Diamond, P.; Smethurst, S.; Fuller, G. A.; Garrington, S. T.; Muxlow, T. W. B.; Spencer, R. E.; Zijlstra, A. A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Purcell, C. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Churchwell, E. B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Diamond, P.; Urquhart, J. S.] CSIRO Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Chandler, C. J.; Shepherd, D. S.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Kurtz, S. E.] Univ Nacl Autonoma Mexico, Ctr Radioastron, Morelia 58090, Michoacan, Mexico.
[Mundy, L. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Dougherty, S. M.] Natl Res Council Canada, Domin Radio Astrophys Observ, Herzberg Inst Astrophys, Penticton, BC V2A 6J9, Canada.
[Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Jackson, J. M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Gledhill, T. R.; Thompson, M. A.] Univ Hertfordshire, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Marti, J.] Univ Jaen, Dept Fis, Escuela Politecn Super Jaen, Jaen 23071, Spain.
[Moore, T. J. T.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Pandian, J. D.] Indian Inst Space Sci & Technol, Trivandrum 695547, Kerala, India.
[Paredes, J. M.] Univ Barcelona UB IEEC, Dept Astron & Meteorol, Barcelona 08028, Spain.
[Paredes, J. M.] Univ Barcelona UB IEEC, ICC, Barcelona 08028, Spain.
[Shepherd, D. S.] Sq Kilometer Array Africa, ZA-7405 Pinelands, South Africa.
[Umana, G.] Osserv Astrofis Catania, I-95123 Catania, Italy.
[Urquhart, J. S.] Max Planck Inst Radio Astron, D-53010 Bonn, Germany.
RP Hoare, MG (reprint author), Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
EM m.g.hoare@leeds.ac.uk
RI Goldsmith, Paul/H-3159-2016;
OI Muxlow, Thomas/0000-0001-5797-8796; Umana, Grazia/0000-0002-6972-8388;
Purcell, Cormac/0000-0002-7491-7386; Paredes, Josep
M./0000-0002-1566-9044
NR 133
TC 46
Z9 46
U1 2
U2 17
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2012
VL 124
IS 919
BP 939
EP 955
DI 10.1086/668058
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016WV
UT WOS:000309551400004
ER
PT J
AU Kinemuchi, K
Barclay, T
Fanelli, M
Pepper, J
Still, M
Howell, SB
AF Kinemuchi, K.
Barclay, T.
Fanelli, M.
Pepper, J.
Still, M.
Howell, Steve B.
TI Demystifying Kepler Data: A Primer for Systematic Artifact Mitigation
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID RED GIANT; INITIAL CHARACTERISTICS; HIERARCHICAL TRIPLE; CADENCE DATA;
STARS. II.; VARIABILITY; SCIENCE; MISSION; PERFORMANCE; ROTATION
AB The Kepler spacecraft has collected data of high photometric precision and cadence almost continuously since operations began on 2009 May 2. Primarily designed to detect planetary transits and asteroseismological signals from solar-like stars, Kepler has provided high-quality data for many areas of investigation. Unconditioned simple aperture time-series photometry is, however, affected by systematic structure. Examples of these systematics include differential velocity aberration, thermal gradients across the spacecraft, and pointing variations. While exhibiting some impact on Kepler's primary science, these systematics can critically handicap potentially ground-breaking scientific gains in other astrophysical areas, especially over long timescales greater than 10 days. As the data archive grows to provide light curves for 10(5) stars of many years in length, Kepler will only fulfill its broad potential for stellar astrophysics if these systematics are understood and mitigated. Post-launch developments in the Kepler archive, data reduction pipeline and open source data analysis software have helped to remove or reduce systematic artifacts. This paper provides a conceptual primer to help users of the Kepler data archive understand and recognize systematic artifacts within light curves and some methods for their removal. Specific examples of artifact mitigation are provided using data available within the archive. Through the methods defined here, the Kepler community will find a road map to maximizing the quality and employment of the Kepler legacy archive.
C1 [Kinemuchi, K.; Barclay, T.; Fanelli, M.; Still, M.] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Kinemuchi, K.; Barclay, T.; Fanelli, M.; Still, M.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pepper, J.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
RP Kinemuchi, K (reprint author), Bay Area Environm Res Inst, Mail Stop 244-30, Moffett Field, CA 94035 USA.
EM karen.kinemuchi@nasa.gov
OI Pepper, Joshua/0000-0002-3827-8417
FU NASA's Science Mission Directorate; NASA [NNX09AR96A, NAS5-26555]; NASA
Office of Space Science [NNX09AF08G]
FX Funding for the Kepler mission is provided by NASA's Science Mission
Directorate. The Kepler Guest Observer Office is funded through NASA
co-operative agreement NNX09AR96A. All of the data presented in this
article were obtained from the Mukulski Archive for Space Telescopes
(MAST). STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for
MAST for non-HST data is provided by the NASA Office of Space Science
via grant NNX09AF08G and by other grants and contracts.
NR 42
TC 35
Z9 35
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2012
VL 124
IS 919
BP 963
EP 984
DI 10.1086/667603
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016WV
UT WOS:000309551400006
ER
PT J
AU Stumpe, MC
Smith, JC
Van Cleve, JE
Twicken, JD
Barclay, TS
Fanelli, MN
Girouard, FR
Jenkins, JM
Kolodziejczak, JJ
McCauliff, SD
Morris, RL
AF Stumpe, Martin C.
Smith, Jeffrey C.
Van Cleve, Jeffrey E.
Twicken, Joseph D.
Barclay, Thomas S.
Fanelli, Michael N.
Girouard, Forrest R.
Jenkins, Jon M.
Kolodziejczak, Jeffery J.
McCauliff, Sean D.
Morris, Robert L.
TI Kepler Presearch Data Conditioning I-Architecture and Algorithms for
Error Correction in Kepler Light Curves
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID SUN-LIKE STAR; NGC 6811; PLANETS; MISSION; SCIENCE; DETECTABILITY;
SYSTEM
AB Kepler provides light curves of 156,000 stars with unprecedented precision. However, the raw data as they come from the spacecraft contain significant systematic and stochastic errors. These errors, which include discontinuities, systematic trends, and outliers, obscure the astrophysical signals in the light curves. To correct these errors is the task of the Presearch Data Conditioning (PDC) module of the Kepler data analysis pipeline. The original version of PDC in Kepler did not meet the extremely high performance requirements for the detection of miniscule planet transits or highly accurate analysis of stellar activity and rotation. One particular deficiency was that astrophysical features were often removed as a side effect of the removal of errors. In this article we introduce the completely new and significantly improved version of PDC which was implemented in Kepler SOC version 8.0. This new PDC version, which utilizes a Bayesian approach for removal of systematics, reliably corrects errors in the light curves while at the same time preserving planet transits and other astrophysically interesting signals. We describe the architecture and the algorithms of this new PDC module, show typical errors encountered in Kepler data, and illustrate the corrections using real light curve examples.
C1 [Stumpe, Martin C.; Smith, Jeffrey C.; Van Cleve, Jeffrey E.; Twicken, Joseph D.; Barclay, Thomas S.; Fanelli, Michael N.; Girouard, Forrest R.; Jenkins, Jon M.; McCauliff, Sean D.; Morris, Robert L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kolodziejczak, Jeffery J.] Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Stumpe, MC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM martin.stumpe@nasa.gov
FU NASA's Science Mission Directorate
FX Funding for this Discovery Mission is provided by NASA's Science Mission
Directorate. We thank the thousands of people whose efforts made
Kepler's grand voyage of discovery possible. We especially thank the
Kepler SOC staff who helped design, build, and operate the Kepler
Science Porcessing Pipeline for putting their hearts into this endeavor.
NR 35
TC 126
Z9 126
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2012
VL 124
IS 919
BP 985
EP 999
DI 10.1086/667698
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016WV
UT WOS:000309551400007
ER
PT J
AU Smith, JC
Stumpe, MC
Van Cleve, JE
Jenkins, JM
Barclay, TS
Fanelli, MN
Girouard, FR
Kolodziejczak, JJ
McCauliff, SD
Morris, RL
Twicken, JD
AF Smith, Jeffrey C.
Stumpe, Martin C.
Van Cleve, Jeffrey E.
Jenkins, Jon M.
Barclay, Thomas S.
Fanelli, Michael N.
Girouard, Forrest R.
Kolodziejczak, Jeffery J.
McCauliff, Sean D.
Morris, Robert L.
Twicken, Joseph D.
TI Kepler Presearch Data Conditioning II - A Bayesian Approach to
Systematic Error Correction
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID LIGHT CURVES; PLANETS
AB With the unprecedented photometric precision of the Kepler spacecraft, significant systematic and stochastic errors on transit signal levels are observable in the Kepler photometric data. These errors, which include discontinuities, outliers, systematic trends, and other instrumental signatures, obscure astrophysical signals. The presearch data conditioning (PDC) module of the Kepler data analysis pipeline tries to remove these errors while preserving planet transits and other astrophysically interesting signals. The completely new noise and stellar variability regime observed in Kepler data poses a significant problem to standard cotrending methods. Variable stars are often of particular astrophysical interest, so the preservation of their signals is of significant importance to the astrophysical community. We present a Bayesian maximum a posteriori (MAP) approach, where a subset of highly correlated and quiet stars is used to generate a cotrending basis vector set, which is in turn used to establish a range of "reasonable" robust fit parameters. These robust fit parameters are then used to generate a Bayesian prior and a Bayesian posterior probability distribution function (PDF) which, when maximized, finds the best fit that simultaneously removes systematic effects while reducing the signal distortion and noise injection that commonly afflicts simple least-squares (LS) fitting. A numerical and empirical approach is taken where the Bayesian prior PDFs are generated from fits to the light-curve distributions themselves.
C1 [Smith, Jeffrey C.; Stumpe, Martin C.; Van Cleve, Jeffrey E.; Jenkins, Jon M.; Barclay, Thomas S.; Fanelli, Michael N.; Girouard, Forrest R.; McCauliff, Sean D.; Morris, Robert L.; Twicken, Joseph D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Smith, Jeffrey C.; Stumpe, Martin C.; Van Cleve, Jeffrey E.; Jenkins, Jon M.; Morris, Robert L.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA.
[Barclay, Thomas S.; Fanelli, Michael N.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Girouard, Forrest R.; McCauliff, Sean D.] Orbital Sci Corp, Dulles, VA 20166 USA.
[Kolodziejczak, Jeffery J.] Marshall Space Flight Ctr, Huntsville, AL 25812 USA.
RP Smith, JC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jeffrey.smith@nasa.gov
FU NASA's Science Mission Directorate
FX Funding for this Discovery Mission is provided by NASA's Science Mission
Directorate. We thank the thousands of people whose efforts made
Kepler's grand voyage of discovery possible. The Kepler Science Office
and Science Working Group work diligently in analyzing data products and
have provided great insight into data reduction methods and data
processing. We especially want to thank the Kepler SOC staff who helped
design, build, and operate the Kepler Science Pipeline for putting their
hearts into this endeavor. The authors would also like to thank the very
productive conversations we have had with the Suzanne Aigrain group at
Oxford University, especially Stephen Reece, Stephen Roberts, and Amy
McQuillan.
NR 22
TC 148
Z9 148
U1 0
U2 6
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2012
VL 124
IS 919
BP 1000
EP 1014
DI 10.1086/667697
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016WV
UT WOS:000309551400008
ER
PT J
AU Chen, F
Weber, KT
Schnase, JL
AF Chen, Fang
Weber, Keith T.
Schnase, John L.
TI Assessing the Success of Postfire Reseeding in Semiarid Rangelands Using
Terra MODIS
SO RANGELAND ECOLOGY & MANAGEMENT
LA English
DT Article
DE fPAR; Idaho; rehabilitation; remote sensing; wildfire
ID PHOTOSYNTHETICALLY ACTIVE RADIATION; NORTH-CENTRAL WASHINGTON;
RESTORATION SUCCESS; LEAF-AREA; LONG-TERM; FIRE; FRACTION; WILDFIRE;
EROSION; FERTILIZATION
AB Successful postfire reseeding efforts can aid rangeland ecosystem recovery by rapidly establishing a desired plant community and thereby reducing the likelihood of infestation by invasive plants. Although the success of postfire remediation is critical, few efforts have been made to leverage existing geospatial technologies to develop methodologies to assess reseeding success following a fire. In this study, Terra Moderate Resolution Imaging Spectroradiometer (MODIS) satellite data were used to improve the capacity to assess postfire reseeding rehabilitation efforts, with particular emphasis on the semiarid rangelands of Idaho. Analysis of MODIS data demonstrated a positive effect of reseeding on rangeland ecosystem recovery, as well as differences in vegetation between reseeded areas and burned areas where no reseeding had occurred (P < 0.05). We conclude that MODIS provides useful data to assess the success of postfire reseeding.
C1 [Chen, Fang; Weber, Keith T.] Idaho State Univ, GIS Training & Res Ctr, Pocatello, ID 83209 USA.
[Schnase, John L.] NASA, Goddard Space Flight Ctr, Off Computat & Informat Sci & Technol, Greenbelt, MD 20771 USA.
RP Chen, F (reprint author), Idaho State Univ, GIS Training & Res Ctr, 921 S 8th Ave,Stop 8104, Pocatello, ID 83209 USA.
EM chenfang@isu.edu
FU National Aeronautics and Space Administration Idaho Space Grant
Consortium [FPK100-SB-004]; National Aeronautics and Space
Administration Goddard Space Flight Center [NNX08A090G]
FX This study was made possible by grants from the National Aeronautics and
Space Administration Idaho Space Grant Consortium (subaward:
FPK100-SB-004) and the National Aeronautics and Space Administration
Goddard Space Flight Center (NNX08A090G).
NR 43
TC 1
Z9 2
U1 2
U2 11
PU SOC RANGE MANAGEMENT
PI LAKEWOOD
PA 445 UNION BLVD, STE 230, LAKEWOOD, CO 80228-1259 USA
SN 1550-7424
J9 RANGELAND ECOL MANAG
JI Rangel. Ecol. Manag.
PD SEP
PY 2012
VL 65
IS 5
BP 468
EP 474
DI 10.2111/REM-D-11-00156.1
PG 7
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 015IJ
UT WOS:000309439300004
ER
PT J
AU Yoonessi, M
Shi, Y
Scheiman, DA
Lebron-Colon, M
Tigelaar, DM
Weiss, RA
Meador, MA
AF Yoonessi, Mitra
Shi, Ying
Scheiman, Daniel A.
Lebron-Colon, Marisabel
Tigelaar, Dean M.
Weiss, R. A.
Meador, Michael A.
TI Graphene Polyimide Nanocomposites; Thermal, Mechanical, and
High-Temperature Shape Memory Effects
SO ACS NANO
LA English
DT Article
DE graphene; polyimide nanocomposites; shape memory polymers; mechanical
properties; thermal stability; exfoliation
ID WALL CARBON NANOTUBES; FUNCTIONALIZED GRAPHENE; ELASTIC PROPERTIES;
SINGLE; SHEETS; FILMS; GRAPHITE; POLYMERS; BEHAVIOR
AB Flexible graphene polyimide nanocomposites (0.1-4 wt %) with superior mechanical properties over those of neat polyimide resin have been prepared by solution blending. Imide moieties were grafted to amine-functionalized graphene using a step-by-step condensation and thermal imidization method. The imide-functionalized graphene exhibited excellent compatibility with N-methyl-2-pyrrolidone. The dynamic storage moduli of the graphene polyimide nanocomposites increased linearly with increasing graphene content for both unmodified graphene and imidized graphene. Moduli of the imidized graphene nanocomposites were 25-30% higher than those of unmodified graphene nanocomposites. Both neat polyimide and polyimide nanocomposites exhibited shape memory effects with a triggering temperature of 230 degrees C. where addition of graphene improved the recovery rate. Addition of graphene improved thermal stability of the polyimide nanocomposites for both graphene and modified graphene.
C1 [Yoonessi, Mitra; Tigelaar, Dean M.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Scheiman, Daniel A.] ASRC, Cleveland, OH 44135 USA.
[Lebron-Colon, Marisabel; Meador, Michael A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Shi, Ying; Weiss, R. A.] Univ Akron, Dept Polymer Engn, Akron, OH 44325 USA.
RP Yoonessi, M (reprint author), Ohio Aerosp Inst, Cleveland, OH 44142 USA.
EM mitra.yoonessi@gmail.com
FU NASA [NNC07BA13B]
FX Funding for this research was provided by the Subsonics Fixed Wing
Project, Fundamental Aeronautics Program under NASA Contract NNC07BA13B.
C. Chuang Is thanked for helpful suggestions and insights on polyimide
chemistry. D. Hull of NASA GRC and Wayne Jennings of Case Western
Reserve University are thanked for TEM and XPS support, respectively.
NR 32
TC 109
Z9 113
U1 26
U2 309
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1936-0851
EI 1936-086X
J9 ACS NANO
JI ACS Nano
PD SEP
PY 2012
VL 6
IS 9
BP 7644
EP 7655
DI 10.1021/nn302871y
PG 12
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 009QP
UT WOS:000309040600011
PM 22931435
ER
PT J
AU Gong, Y
Andrews, L
Bauschlicher, CW
AF Gong, Yu
Andrews, Lester
Bauschlicher, Charles W., Jr.
TI Formation of Metal Oxyfluorides from Specific Metal Reactions with
Oxygen Difluoride: Infrared Spectroscopic and Theoretical Investigations
of the OScF2 Radical and OScF with Terminal Single and Triple Sc?O Bonds
SO CHEMISTRY-A EUROPEAN JOURNAL
LA English
DT Article
DE density functional calculations; matrix isolation; oxygen; radicals;
scandium
ID DENSITY-FUNCTIONAL CALCULATIONS; HARMONIC VIBRATIONAL FREQUENCIES;
GAUSSIAN-BASIS SETS; SOLID ARGON; ELECTRONIC-STRUCTURE;
TRANSITION-METALS; MATRIX-ISOLATION; PHOTOELECTRON-SPECTROSCOPY;
CHALCOGENIDO COMPLEXES; MOLECULAR CALCULATIONS
AB The scandium oxydifluoride free radical, OScF2, is produced by the spontaneous, specific reaction of laser ablated Sc atoms with OF2 in solid argon and characterized by using matrix infrared spectroscopy and theoretical calculations. The OScF2 molecule is predicted to have C2v symmetry and a 2B2 ground state with an unpaired electron located primarily on the terminal oxygen atom, which makes it a scandium difluoride molecule coordinated by a neutral oxygen atom radical in forming the Sc?O single bond. The closed shell singlet OScF molecule with an obtuse bent geometry has a much shorter Sc?O bond of 1.682 angstrom than that of the OScF2 radical (1.938 angstrom) on the basis of B3LYP calculations. The Sc?O bond in OScF consists of two covalent bonds and a dative bond in which the oxygen 2pp lone pair donates electron density into an empty Sc 3d orbital thus forming a triple oxo bond. Density functional calculations suggest it is highly exothermic for fluorine transfer from OF2 to scandium, which favors the formation of the OScF2 radical species as well as the OScF molecule after fluorine loss.
C1 [Gong, Yu; Andrews, Lester] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
[Bauschlicher, Charles W., Jr.] NASA, Entry Syst & Technol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Andrews, L (reprint author), Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
EM lsa@virginia.edu
FU DOE [DE-SC0001034]
FX This work was supported by DOE Grant DE-SC0001034 to L.A.
NR 64
TC 2
Z9 2
U1 4
U2 19
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 0947-6539
J9 CHEM-EUR J
JI Chem.-Eur. J.
PD SEP
PY 2012
VL 18
IS 39
BP 12446
EP 12451
DI 10.1002/chem.201201005
PG 6
WC Chemistry, Multidisciplinary
SC Chemistry
GA 007HI
UT WOS:000308879000034
PM 22907675
ER
PT J
AU Elsila, JE
Charnley, SB
Burton, AS
Glavin, DP
Dworkin, JP
AF Elsila, Jamie E.
Charnley, Steven B.
Burton, Aaron S.
Glavin, Daniel P.
Dworkin, Jason P.
TI Compound-specific carbon, nitrogen, and hydrogen isotopic ratios for
amino acids in CM and CR chondrites and their use in evaluating
potential formation pathways
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Review
ID INTERSTELLAR ICE ANALOGS; EARLY SOLAR-SYSTEM; INTERPLANETARY DUST
PARTICLES; WAVE ROTATIONAL SPECTRUM; MURCHISON METEORITE;
ORGANIC-MATTER; MASS-SPECTROMETRY; MOLECULAR CLOUDS; DEUTERIUM
ENRICHMENT; OBSERVATIONAL TESTS
AB Stable hydrogen, carbon, and nitrogen isotopic ratios (dD, d13C, and d15N) of organic compounds can reveal information about their origin and formation pathways. Several formation mechanisms and environments have been postulated for the amino acids detected in carbonaceous chondrites. As each proposed mechanism utilizes different precursor molecules, the isotopic signatures of the resulting amino acids may indicate the most likely of these pathways. We have applied gas chromatography with mass spectrometry and combustion isotope ratio mass spectrometry to measure the compound-specific C, N, and H stable isotopic ratios of amino acids from seven CM and CR carbonaceous chondrites: CM1/2 Allan Hills (ALH) 83100, CM2 Murchison, CM2 Lewis Cliff (LEW) 90500, CM2 Lonewolf Nunataks (LON) 94101, CR2 Graves Nunataks (GRA) 95229, CR2 Elephant Moraine (EET) 92042, and CR3 Queen Alexandra Range (QUE) 99177. We compare the isotopic compositions of amino acids in these meteorites with predictions of expected isotopic enrichments from potential formation pathways. We observe trends of decreasing d13C and increasing dD with increasing carbon number in the a-H, a-NH2 amino acids that correspond to predictions made for formation via Strecker-cyanohydrin synthesis. We also observe light d13C signatures for beta-alanine, which may indicate either formation via Michael addition or via a pathway that forms primarily small, straight-chain, amine-terminal amino acids (n-?-amino acids). Higher deuterium enrichments are observed in a-methyl amino acids, indicating formation of these amino acids or their precursors in cold interstellar or nebular environments. Finally, individual amino acids are more enriched in deuterium in CR chondrites than in CM chondrites, reflecting different parent-body chemistry.
C1 [Elsila, Jamie E.; Charnley, Steven B.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Elsila, Jamie E.; Charnley, Steven B.; Glavin, Daniel P.; Dworkin, Jason P.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Burton, Aaron S.] NASA, Postdoctoral Program, Greenbelt, MD 20771 USA.
RP Elsila, JE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jamie.elsila@nasa.gov
RI Elsila, Jamie/C-9952-2012; Burton, Aaron/H-2212-2011; 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 NASA Astrobiology Institute; Goddard Center for Astrobiology; NASA; NASA
at the Goddard Space Flight Center
FX We thank the Smithsonian National Museum of Natural History and the
Meteorite Working Group for the meteorite samples analyzed in this
study. This work was supported by the NASA Astrobiology Institute and
the Goddard Center for Astrobiology, as well as NASA's Cosmochemistry
and Origins of Solar Systems Programs. A.S.B. acknowledges support from
the NASA Postdoctoral Program at the Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. We thank C. Alexander for useful discussion; M. Callahan, M.
Martin, and J. Stern for both useful discussion and technical
assistance; and two anonymous reviewers for careful review of this
manuscript.
NR 106
TC 22
Z9 23
U1 1
U2 49
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 SEP
PY 2012
VL 47
IS 9
BP 1517
EP 1536
DI 10.1111/j.1945-5100.2012.01415.x
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 012KC
UT WOS:000309234000008
ER
PT J
AU Greene, CH
Monger, BC
McGarry, LP
Connelly, MD
Schnepf, NR
Pershing, AJ
Belkin, IM
Fratantoni, PS
Mountain, DG
Pickart, RS
Ji, RB
Bisagni, JJ
Chen, CS
Hakkinen, SMA
Haidvogel, DB
Wang, J
Head, E
Smith, P
Conversi, A
AF Greene, Charles H.
Monger, Bruce C.
McGarry, Louise P.
Connelly, Matthew D.
Schnepf, Neesha R.
Pershing, Andrew J.
Belkin, Igor M.
Fratantoni, Paula S.
Mountain, David G.
Pickart, Robert S.
Ji, Rubao
Bisagni, James J.
Chen, Changsheng
Hakkinen, Sirpa M. A.
Haidvogel, Dale B.
Wang, Jia
Head, Erica
Smith, Peter
Conversi, Alessandra
CA Marine Ecosyst Responses Climate N
TI Recent Arctic Climate Change and Its Remote Forcing of Northwest
Atlantic Shelf Ecosystems
SO OCEANOGRAPHY
LA English
DT Article
ID VARIABILITY; OCEAN; WATER; MAINE; ATMOSPHERE; IMPACTS; GULF
AB During recent decades, historically unprecedented changes have been observed in the Arctic as climate warming has increased precipitation, river discharge, and glacial as well as sea ice melting. Additionally, shifts in the Arctic's atmospheric pressure field have altered surface winds, ocean circulation, and freshwater storage in the Beaufort Gyre. These processes have resulted in variable patterns of freshwater export from the Arctic Ocean, including the emergence of great salinity anomalies propagating throughout the North Atlantic. Here, we link these variable patterns of freshwater export from the Arctic Ocean to the regime shifts observed in Northwest Atlantic shelf ecosystems. Specifically, we hypothesize that the corresponding salinity anomalies, both negative and positive, alter the timing and extent of water-column stratification, thereby impacting the production and seasonal cycles of phytoplankton, zooplankton, and higher-trophic-level consumers. Should this hypothesis hold up to critical evaluation, it has the potential to fundamentally alter our current understanding of the processes forcing the dynamics of Northwest Atlantic shelf ecosystems.
C1 [Greene, Charles H.; McGarry, Louise P.; Connelly, Matthew D.; Schnepf, Neesha R.] Cornell Univ, Ocean Resources & Ecosyst Program, Ithaca, NY 14853 USA.
[Pershing, Andrew J.] Gulf Maine Res Inst, Portland, ME USA.
[Pershing, Andrew J.] Univ Maine, Sch Marine Sci, Orono, ME USA.
[Belkin, Igor M.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA.
[Fratantoni, Paula S.] NOAA, Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, Woods Hole, MA 02543 USA.
[Pickart, Robert S.] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA.
[Ji, Rubao] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA.
[Bisagni, James J.; Chen, Changsheng] Univ Massachusetts Dartmouth, Sch Marine Sci & Technol, New Bedford, MA USA.
[Hakkinen, Sirpa M. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Haidvogel, Dale B.] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA.
[Wang, Jia] NOAA, Great Lakes Environm Res Lab, Ann Arbor, MI 48105 USA.
[Head, Erica; Smith, Peter] Fisheries & Oceans Canada, Bedford Inst Oceanog, Dept Fisheries & Oceans, Dartmouth, NS B2Y 4A2, Canada.
[Conversi, Alessandra] Italian Natl Res Council, Inst Marine Sci, La Spezia, Italy.
[Conversi, Alessandra] Univ Plymouth, Inst Marine, Plymouth PL4 8AA, Devon, England.
[Conversi, Alessandra] Sir Alister Hardy Fdn Ocean Sci, Plymouth, Devon, England.
RP Greene, CH (reprint author), Cornell Univ, Ocean Resources & Ecosyst Program, Ithaca, NY 14853 USA.
EM chg2@cornell.edu
RI CNR, Ismar/P-1247-2014; Ji, Rubao/I-1970-2015
OI CNR, Ismar/0000-0001-5351-1486; Ji, Rubao/0000-0002-8839-5427
FU National Science Foundation as part of the Regional and Pan-Regional
Synthesis Phases of the US Global Ocean Ecosystem (GLOBEC) Program
FX We gratefully acknowledge the assistance of Andrey Proshutinsky in
clarifying the complexity and unusual behavior of the Arctic Ocean,
especially during recent years. We also thank the Gulf of Maine Research
Institute, Cornell University's Shoals Marine Laboratory, and the
University of Washington's Friday Harbor Laboratories (FHL) for hosting
the research workshops at which the ideas in this paper were developed.
CHG thanks FHL for hosting him as a Whiteley Center Scholar during the
preparation of this manuscript. Funding for this research was provided
by the National Science Foundation as part of the Regional and
Pan-Regional Synthesis Phases of the US Global Ocean Ecosystem (GLOBEC)
Program.
NR 34
TC 12
Z9 12
U1 4
U2 61
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD SEP
PY 2012
VL 25
IS 3
SI SI
BP 208
EP 213
PG 6
WC Oceanography
SC Oceanography
GA 005UC
UT WOS:000308774600033
ER
PT J
AU Abbas, MM
Tankosic, D
LeClair, AC
Spann, JF
AF Abbas, M. M.
Tankosic, D.
LeClair, A. C.
Spann, J. F.
TI CHARGING OF DUST GRAINS IN ASTROPHYSICAL ENVIRONMENTS BY SECONDARY
ELECTRON EMISSIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; Moon
ID LUNAR DUST; INTERSTELLAR DUST; PHOTOELECTRON EMISSION; PARTICLES; SIZE;
SPACE; INSULATORS; RADIATION; ANALOGS; ENERGY
AB The dominant charging processes in various astrophysical environments are considered to be by photoelectric emissions with radiation from nearby stars and secondary electron emissions (SEE) by impact of electrons in a medium with sufficiently high energies. The charging of bulk materials with planar surfaces by SEE with electron impact appears to be well understood with theoretical expressions as well as by experimental techniques. However, the charging of submicron/micron-size dust grains by SEE with sufficiently high-energy electrons is a complex process, and is a function of electron energies, the electron current, and the grain size, and the charge or the surface potential. Development of viable theoretical models and acquisition of experimental data for charging properties of micron-size dust grains are still in the early stages. This paper focuses on SEE charging properties of individual micron-size dust grains by low-energy electron impact, obtained from laboratory measurements on an experimental facility based on an electrodynamic balance. The measurements of SEE yields of positively charged dust grains indicate the yields increase with decreasing grain size and the equilibrium surface potentials showing generally linear size dependence. These experimental results are generally in agreement with several independent experimental and analytical model studies in the literature, with the exception of a recently published paper which is in fundamental conflict with our studies as well as with several other experimental and theoretical studies. The sources and causes of this conflict are critically examined and discussed in this paper.
C1 [Abbas, M. M.; LeClair, A. C.; Spann, J. F.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Tankosic, D.] NASA, George C Marshall Space Flight Ctr, NPP, Huntsville, AL 35805 USA.
RP Abbas, MM (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM Mian.M.Abbas@nasa.gov
FU Science Directorate at NASA Marshall Space Flight Center
FX This work was supported by the Science Directorate at NASA Marshall
Space Flight Center, and we are grateful to Dr. D. L. Gallagher, and Dr.
Robert Sheldon for helpful comments during the course of this work.
Sincere thanks are also due to Alvin Cantrell and Ed West for generous
help in carrying out the experimental program.
NR 45
TC 1
Z9 1
U1 2
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 41
DI 10.1088/0004-637X/756/1/41
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300041
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Antolini, E
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bottacini, E
Brandt, TJ
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Cecchi, C
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
D'Ammando, F
de Angelis, A
de Palma, F
Dermer, CD
Silva, EDE
Drell, PS
Drlica-Wagner, A
Enoto, T
Falletti, L
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fukazawa, Y
Fukui, Y
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hayashi, K
Horan, D
Hou, X
Hughes, RE
Jackson, MS
Johannesson, G
Johnson, AS
Kamae, T
Katagiri, H
Kataoka, J
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Lee, SH
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Makishima, K
Mazziotta, MN
Mehault, J
Mitthumsiri, W
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Naumann-Godo, M
Nishino, S
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Orienti, M
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pelassa, V
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Razzano, M
Reimer, A
Reimer, O
Roth, M
Sadrozinski, HFW
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Strong, AW
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JG
Thayer, JB
Tibolla, O
Tinivella, M
Torres, DF
Tramacere, A
Troja, E
Uchiyama, Y
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Wang, P
Winer, BL
Wood, KS
Yang, Z
Zimmer, S
AF Ackermann, M.
Ajello, M.
Allafort, A.
Antolini, E.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Cecchi, C.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Enoto, T.
Falletti, L.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fukazawa, Y.
Fukui, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hayashi, K.
Horan, D.
Hou, X.
Hughes, R. E.
Jackson, M. S.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kerr, M.
Knodlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Lee, S. -H.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Makishima, K.
Mazziotta, M. N.
Mehault, J.
Mitthumsiri, W.
Moiseev, A. A.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Naumann-Godo, M.
Nishino, S.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Orienti, M.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Razzano, M.
Reimer, A.
Reimer, O.
Roth, M.
Sadrozinski, H. F. -W.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strong, A. W.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Tibolla, O.
Tinivella, M.
Torres, D. F.
Tramacere, A.
Troja, E.
Uchiyama, Y.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Zimmer, S.
TI GAMMA-RAY OBSERVATIONS OF THE ORION MOLECULAR CLOUDS WITH THE FERMI
LARGE AREA TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: ISM; ISM: clouds; ISM: general; ISM: individual objects
(Orion A and Orion B)
ID CO-TO-H-2 CONVERSION FACTOR; ALL-SKY SURVEY; ROTATIONAL-EXCITATION;
CARBON-MONOXIDE; COSMIC-RAY; CO SURVEY; DARK CLOUDS; MILKY-WAY; X-RAY;
METALLICITY DEPENDENCE
AB We report on the gamma-ray observations of giant molecular clouds Orion A and B with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. The gamma-ray emission in the energy band between similar to 100 MeV and similar to 100 GeV is predicted to trace the gas mass distribution in the clouds through nuclear interactions between the Galactic cosmic rays (CRs) and interstellar gas. The gamma-ray production cross-section for the nuclear interaction is known to similar to 10% precision which makes the LAT a powerful tool to measure the gas mass column density distribution of molecular clouds for a known CR intensity. We present here such distributions for Orion A and B, and correlate them with those of the velocity-integrated CO intensity (W-CO) at a 1 degrees x 1 degrees pixel level. The correlation is found to be linear over a W-CO range of similar to 10-fold when divided in three regions, suggesting penetration of nuclear CRs to most of the cloud volumes. The W-CO-to-mass conversion factor, X-CO, is found to be similar to 2.3 x 10(20) cm(-2) (K km s(-1))(-1) for the high-longitude part of Orion A (l > 212 degrees), similar to 1.7 times higher than similar to 1.3 x 10(20) found for the rest of Orion A and B. We interpret the apparent high XCO in the high-longitude region of Orion A in the light of recent works proposing a nonlinear relation between H-2 and CO densities in the diffuse molecular gas. W-CO decreases faster than the H-2 column density in the region making the gas "darker" to W-CO.
C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Antolini, E.; Bonamente, E.; Cecchi, C.; D'Ammando, F.; Germani, S.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, CNRS,CEA IRFU,Lab AIM, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Brandt, T. J.; Knodlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Brandt, T. J.; Knodlseder, J.] Univ Toulouse, IRAP, UPS OMP, GAHEC, Toulouse, France.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] M Merlin Univ, Dipartimento Fis, 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.
[Bruel, P.; Fegan, S. J.; Horan, D.] CNRS IN2P3, Ecole Polytech, Lab Leprince Ringuet, Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Chekhtman, A.; Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Ciprini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Cohen-Tanugi, J.; Falletti, L.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[Conrad, J.; Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy.
[D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ferrara, E. C.; Harding, A. K.; Moiseev, A. A.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Nishino, S.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Fukui, Y.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.; Pelassa, V.] Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hou, X.] Univ Bordeaux 1, CNRS IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Dept Phys, Columbus, OH 43210 USA.
[Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Tokyo, Tokyo 1698555, Japan.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Makishima, K.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Moiseev, A. A.] Ctr Res & Explorat Space Sci & Technol CRESST, 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.
[Morselli, A.; Ohno, M.; 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.
[Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[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.; Sadrozinski, H. F. -W.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Razzano, M.; Sadrozinski, H. F. -W.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Reimer, A.; Reimer, O.; Roth, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.; Roth, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Torres, D. F.] Inst Catalana Recerca & Estudis Avancats ICREA, Barcelona, Spain.
[Tramacere, A.; Vianello, G.] Consorzio Interuniv Fis Spaziale CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM kamae@slac.stanford.edu; oxon@mac.com
RI giglietto, nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Harding,
Alice/D-3160-2012; Reimer, Olaf/A-3117-2013; Ozaki,
Masanobu/K-1165-2013; Johannesson, Gudlaugur/O-8741-2015; Loparco,
Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Sgro,
Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007
OI Tramacere, Andrea/0000-0002-8186-3793; Baldini,
Luca/0000-0002-9785-7726; De Angelis, Alessandro/0000-0002-3288-2517;
Caraveo, Patrizia/0000-0003-2478-8018; Sgro',
Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864;
Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins,
Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094;
Giroletti, Marcello/0000-0002-8657-8852; Berenji,
Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495;
giglietto, nicola/0000-0002-9021-2888; Morselli,
Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Johannesson,
Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Giordano, Francesco/0000-0002-8651-2394;
Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X
FU K. A. Wallenberg Foundation; Istituto Nazionale di Astrofisica in Italy;
Centre National d'Etudes Spatiales in France
FX Royal Swedish Academy of Sciences Research Fellow, funded 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 96
TC 17
Z9 17
U1 0
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 4
DI 10.1088/0004-637X/756/1/4
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300004
ER
PT J
AU Cheung, CC
Donato, D
Gehrels, N
Sokolovsky, KV
Giroletti, M
AF Cheung, C. C.
Donato, D.
Gehrels, N.
Sokolovsky, K. V.
Giroletti, M.
TI CHANDRA X-RAY OBSERVATIONS OF THE TWO BRIGHTEST UNIDENTIFIED HIGH
GALACTIC LATITUDE FERMI-LAT gamma-RAY SOURCES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; gamma rays: general; pulsars: general; X-rays: general
ID LARGE-AREA TELESCOPE; ALL-SKY SURVEY; MILLISECOND PULSARS; SOURCE
CATALOG; SEYFERT-GALAXIES; 3EG J1835+5918; RADIO GALAXY; SOURCE LIST; B
CATALOG; DISCOVERY
AB We present Chandra ACIS-I X-ray observations of 0FGL J1311.9-3419 and 0FGL J1653.4-0200, the two brightest high Galactic latitude (|b| > 10 degrees) gamma-ray sources from the three-month Fermi Large Area Telescope (LAT) bright source list that are still unidentified. Both were also detected previously by EGRET, and despite dedicated multi-wavelength follow-up, they are still not associated with established classes of gamma-ray emitters like pulsars or radio-loud active galactic nuclei. X-ray sources found in the ACIS-I fields of view are cataloged, and their basic properties are determined. These are discussed as candidate counterparts to 0FGL J1311.9-3419 and 0FGL J1653.4-0200, with particular emphasis on the brightest of the 9 and 13 Chandra sources detected within the respective Fermi-LAT 95% confidence regions. Further follow-up studies, including optical photometric and spectroscopic observations, are necessary to identify these X-ray candidate counterparts in order to ultimately reveal the nature of these enigmatic gamma-ray objects.
C1 [Cheung, C. C.; Donato, D.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Donato, D.] CRESST, Greenbelt, MD 20771 USA.
[Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Sokolovsky, K. V.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117810, Russia.
[Sokolovsky, K. V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
RP Cheung, CC (reprint author), USN, Res Lab, Washington, DC 20375 USA.
EM Teddy.Cheung.ctr@nrl.navy.mil; Davide.Donato-1@nasa.gov
RI Sokolovsky, Kirill/D-2246-2015
OI Sokolovsky, Kirill/0000-0001-5991-6863
FU NASA; NASA [DPR S-15633-Y]; National Aeronautics and Space
Administration through Chandra Award [GO0-11022A]; National Aeronautics
Space Administration [NAS8-03060]
FX This work began while C. C. C. was supported by an appointment to the
NASA Postdoctoral Program at Goddard Space Flight Center, administered
by Oak Ridge Associated Universities through a contract with NASA; his
work at NRL is supported in part by NASA DPR S-15633-Y. Support for this
work was partially provided by the National Aeronautics and Space
Administration through Chandra Award Number GO0-11022A (C. C. C. and D.
D.) issued by the Chandra X-ray Observatory Center, which is operated by
the Smithsonian Astrophysical Observatory for and on behalf of the
National Aeronautics Space Administration under contract NAS8-03060.
NR 53
TC 16
Z9 16
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 33
DI 10.1088/0004-637X/756/1/33
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300033
ER
PT J
AU Choi, JY
Shin, IG
Han, C
Udalski, A
Sumi, T
Gould, A
Bozza, V
Dominik, M
Fouque, P
Horne, K
Szymanski, MK
Kubiak, M
Soszynski, I
Pietrzynski, G
Poleski, R
Ulaczyk, K
Pietrukowicz, P
Kozlowski, S
Skowron, J
Wyrzykowski, L
Abe, F
Bennett, DP
Bond, IA
Botzler, CS
Chote, P
Freeman, M
Fukui, A
Furusawa, K
Itow, Y
Kobara, S
Ling, CH
Masuda, K
Matsubara, Y
Miyake, N
Muraki, Y
Ohmori, K
Ohnishi, K
Rattenbury, NJ
Saito, T
Sullivan, DJ
Suzuki, D
Suzuki, K
Sweatman, WL
Takino, S
Tristram, PJ
Wada, K
Yock, PCM
Bramich, DM
Snodgrass, C
Steele, IA
Street, RA
Tsapras, Y
Alsubai, KA
Browne, P
Burgdorf, MJ
Novati, SC
Dodds, P
Dreizler, S
Fang, XS
Grundahl, F
Gu, CH
Hardis, S
Harpsoe, K
Hinse, TC
Hornstrup, A
Hundertmark, M
Jessen-Hansen, J
Jorgensen, UG
Kains, N
Kerins, E
Liebig, C
Lund, M
Lunkkvist, M
Mancini, L
Mathiasen, M
Penny, MT
Rahvar, S
Ricci, D
Scarpetta, G
Skottfelt, J
Southworth, J
Surdej, J
Tregloan-Reed, J
Wambsganss, J
Wertz, O
Almeida, LA
Batista, V
Christie, G
DePoy, DL
Dong, SB
Gaudi, BS
Henderson, C
Jablonski, F
Lee, CU
McCormick, J
McGregor, D
Moorhouse, D
Natusch, T
Ngan, H
Pogge, RW
Tan, TG
Thornley, G
Yee, JC
Albrow, MD
Bachelet, E
Beaulieu, JP
Brillant, S
Cassan, A
Cole, AA
Corrales, E
Coutures, C
Dieters, S
Prester, DD
Donatowicz, J
Greenhill, J
Kubas, D
Marquette, JB
Menzies, JW
Sahu, KC
Zub, M
AF Choi, J. -Y.
Shin, I. -G.
Han, C.
Udalski, A.
Sumi, T.
Gould, A.
Bozza, V.
Dominik, M.
Fouque, P.
Horne, K.
Szymanski, M. K.
Kubiak, M.
Soszynski, I.
Pietrzynski, G.
Poleski, R.
Ulaczyk, K.
Pietrukowicz, P.
Kozlowski, S.
Skowron, J.
Wyrzykowski, L.
Abe, F.
Bennett, D. P.
Bond, I. A.
Botzler, C. S.
Chote, P.
Freeman, M.
Fukui, A.
Furusawa, K.
Itow, Y.
Kobara, S.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Miyake, N.
Muraki, Y.
Ohmori, K.
Ohnishi, K.
Rattenbury, N. J.
Saito, To.
Sullivan, D. J.
Suzuki, D.
Suzuki, K.
Sweatman, W. L.
Takino, S.
Tristram, P. J.
Wada, K.
Yock, P. C. M.
Bramich, D. M.
Snodgrass, C.
Steele, I. A.
Street, R. A.
Tsapras, Y.
Alsubai, K. A.
Browne, P.
Burgdorf, M. J.
Novati, S. Calchi
Dodds, P.
Dreizler, S.
Fang, X. -S.
Grundahl, F.
Gu, C. -H.
Hardis, S.
Harpsoe, K.
Hinse, T. C.
Hornstrup, A.
Hundertmark, M.
Jessen-Hansen, J.
Jorgensen, U. G.
Kains, N.
Kerins, E.
Liebig, C.
Lund, M.
Lunkkvist, M.
Mancini, L.
Mathiasen, M.
Penny, M. T.
Rahvar, S.
Ricci, D.
Scarpetta, G.
Skottfelt, J.
Southworth, J.
Surdej, J.
Tregloan-Reed, J.
Wambsganss, J.
Wertz, O.
Almeida, L. A.
Batista, V.
Christie, G.
DePoy, D. L.
Dong, Subo
Gaudi, B. S.
Henderson, C.
Jablonski, F.
Lee, C. -U.
McCormick, J.
McGregor, D.
Moorhouse, D.
Natusch, T.
Ngan, H.
Pogge, R. W.
Tan, T. -G.
Thornley, G.
Yee, J. C.
Albrow, M. D.
Bachelet, E.
Beaulieu, J. -P.
Brillant, S.
Cassan, A.
Cole, A. A.
Corrales, E.
Coutures, C.
Dieters, S.
Prester, D. Dominis
Donatowicz, J.
Greenhill, J.
Kubas, D.
Marquette, J. -B.
Menzies, J. W.
Sahu, K. C.
Zub, M.
CA OGLE Collaboration
MOA Collaboration
RoboNet Collaboration
MiNDSTEp Consortium
mFun Collaboration
PLANET Collaboration
TI A NEW TYPE OF AMBIGUITY IN THE PLANET AND BINARY INTERPRETATIONS OF
CENTRAL PERTURBATIONS OF HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING
EVENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: bulge; gravitational lensing: micro
ID DIFFERENCE IMAGE-ANALYSIS; JOVIAN-MASS PLANET; GALACTIC BULGE; OPTICAL
DEPTH; EXTRASOLAR PLANETS; LENS IMAGES; CAUSTICS; DISCOVERY; CHANNEL;
SYSTEMS
AB High-magnification microlensing events provide an important channel to detect planets. Perturbations near the peak of a high-magnification event can be produced either by a planet or a binary companion. It is known that central perturbations induced by both types of companions can be generally distinguished due to the essentially different magnification pattern around caustics. In this paper, we present a case of central perturbations for which it is difficult to distinguish the planetary and binary interpretations. The peak of a lensing light curve affected by this perturbation appears to be blunt and flat. For a planetary case, this perturbation occurs when the source trajectory passes the negative perturbation region behind the back end of an arrowhead-shaped central caustic. For a binary case, a similar perturbation occurs for a source trajectory passing through the negative perturbation region between two cusps of an astroid-shaped caustic. We demonstrate the degeneracy for two high-magnification events of OGLE-2011-BLG-0526 and OGLE-2011-BLG-0950/MOA-2011-BLG-336. For OGLE-2011-BLG-0526, the chi(2) difference between the planetary and binary model is similar to 3, implying that the degeneracy is very severe. For OGLE-2011-BLG-0950/MOA-2011-BLG-336, the stellar binary model is formally excluded with Delta chi(2) similar to 105 and the planetary model is preferred. However, it is difficult to claim a planet discovery because systematic residuals of data from the planetary model are larger than the difference between the planetary and binary models. Considering that two events observed during a single season suffer from such a degeneracy, it is expected that central perturbations experiencing this type of degeneracy is common.
C1 [Choi, J. -Y.; Shin, I. -G.; Han, C.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea.
[Udalski, A.; Szymanski, M. K.; Kubiak, M.; Soszynski, I.; Pietrzynski, G.; Poleski, R.; Ulaczyk, K.; Pietrukowicz, P.; Kozlowski, S.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Gould, A.; Skowron, J.; Penny, M. T.; Batista, V.; Gaudi, B. S.; Henderson, C.; McGregor, D.; Pogge, R. W.; Yee, J. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
[Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, I-84081 Baronissi, Salerno, Italy.
[Dominik, M.; Horne, K.; Browne, P.; Dodds, P.; Hundertmark, M.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Fouque, P.; Bachelet, E.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France.
[Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Abe, F.; Furusawa, K.; Itow, Y.; Kobara, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Ohmori, K.; Suzuki, K.; Takino, S.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[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, New Zealand.
[Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand.
[Chote, P.; Sullivan, D. J.; Tristram, P. J.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand.
[Fukui, A.] NAOJ, Okayama Astrophys Observ, Okayama 7190232, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano, Japan.
[Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[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.
[Street, R. A.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England.
[Alsubai, K. A.] Qatar Fdn, Doha, Qatar.
[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; Scarpetta, G.] Ist Int Alti Studi Sci IIASS, Vietri Sul Mare, SA, Italy.
[Dreizler, S.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Fang, X. -S.; Gu, C. -H.] Chinese Acad Sci, Joint Lab Optic Astron, Natl Astron Observ, Yunnan Observ, Kunming 650011, Peoples R China.
[Grundahl, F.; Jessen-Hansen, J.; Lund, M.; Lunkkvist, M.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark.
[Hardis, S.; Harpsoe, K.; Hinse, T. C.; Jorgensen, U. G.; Mathiasen, M.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Harpsoe, K.; Jorgensen, U. G.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Hinse, T. C.; Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon, South Korea.
[Hornstrup, A.] Danmarks Tekn Univ, Inst Rumforskning & Teknol, DK-2100 Copenhagen, Denmark.
[Kains, N.] ESO Headquarters, D-85748 Garching, Germany.
[Kerins, E.; Penny, M. T.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Mancini, L.] Int Inst Adv Sci Studies, I-84019 Vietri Sul Mare, SA, 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.; Wertz, O.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Southworth, J.; Tregloan-Reed, J.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Wambsganss, J.; Zub, M.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany.
[Almeida, L. A.; Jablonski, F.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, SP, Brazil.
[Christie, G.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland, New Zealand.
[DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Dong, Subo] Inst Adv Study, Princeton, NJ 08540 USA.
[McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand.
[Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand.
[Natusch, T.] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand.
[Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, C.; Kubas, D.; Marquette, J. -B.] Inst Astrophys Paris, UMR 7095, UPMC CNRS, F-75014 Paris, France.
[Brillant, S.; Kubas, D.] European So Observ, Santiago 19, Chile.
[Cole, A. A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia.
[Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1040 Vienna, Austria.
[Menzies, J. W.] S African Astron Observ, ZA-7925 Cape Town, South Africa.
[Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Choi, JY (reprint author), Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea.
RI Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012; Almeida,
L./G-7188-2012; Greenhill, John/C-8367-2013; Kozlowski,
Szymon/G-4799-2013; 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013;
Skowron, Jan/M-5186-2014; Hundertmark, Markus/C-6190-2015; Rahvar,
Sohrab/A-9350-2008;
OI Ricci, Davide/0000-0002-9790-0552; Penny, Matthew/0000-0001-7506-5640;
Snodgrass, Colin/0000-0001-9328-2905; Lund, Mikkel
Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571;
Kozlowski, Szymon/0000-0003-4084-880X; Skowron, Jan/0000-0002-2335-1730;
Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Cole,
Andrew/0000-0003-0303-3855
FU Creative Research Initiative Program of the National Research Foundation
of Korea [2009-0081561]; European Research Council under European
Community [246678]; JSPS [JSPS23540339, JSPS19340058]; German Research
Foundation (DFG); Communaute francaise de Belgique Actions de recherche
concertees, Academie universitaire Wallonie-Europe; NPRP [09-476-1-078];
European Union [268421]; Danish Natural Science Foundation; NSF
[AST-1103471]; NASA [NNG04GL51G]; National Science Foundation
[2009068160]; California Institute of Technology (Caltech); NASA through
the Sagan Fellowship Program; KRCF Young Scientist Research Fellowship
Program; Korea Astronomy and Space Science Institute (KASI)
[2012-1-410-02]; [JSPS22403003]; [JSPS23340064]; [JSPS23340044]
FX Work by C. H. was supported by the Creative Research Initiative Program
(2009-0081561) of the National Research Foundation of Korea. 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. The MOA experiment was supported by grants
JSPS22403003 and JSPS23340064. T. S. was supported by the grant
JSPS23340044. Y. Muraki acknowledges support from JSPS grants
JSPS23540339 and JSPS19340058. The MiNDSTEp monitoring campaign is
powered by ARTEMiS (Automated Terrestrial Exoplanet Microlensing Search;
Dominik et al. 2008). M. H. acknowledges support by the German Research
Foundation (DFG). D. R. (boursier FRIA), O.W. (FNRS research fellow),
and J. Surdej acknowledge support from the Communaute francaise de
Belgique Actions de recherche concertees, Academie universitaire
Wallonie-Europe. K. A., D. M. B., M. D., K. H., M. H., C. L., C. S., R.
A. S., and Y. T. are thankful to Qatar National Research Fund (QNRF),
member of Qatar Foundation, for support by grant NPRP 09-476-1-078. C.
S. received funding from the European Union Seventh Framework Programme
(FPT/2007-2013) under grant agreement 268421. This work is based in part
on data collected by MiNDSTEp with the Danish 1.54 m telescope at the
ESO La Silla Observatory. The Danish 1.54 m telescope is operated based
on a grant from the Danish Natural Science Foundation (FNU). A. Gould
and B. S. Gaudi acknowledge support from NSF AST-1103471. B. S. Gaudi,
A. Gould, and R. W. Pogge acknowledge support from NASA grant
NNG04GL51G. Work by J. C. Yee is supported by a National Science
Foundation Graduate Research Fellowship under Grant No. 2009068160. S.
Dong's research was performed under contract with the California
Institute of Technology (Caltech) funded by NASA through the Sagan
Fellowship Program. Research by T. C. H. was carried out under the KRCF
Young Scientist Research Fellowship Program. T. C. H. and C. U. L.
acknowledge the support of Korea Astronomy and Space Science Institute
(KASI) grant 2012-1-410-02. Dr. David Warren provided financial support
for Mt. Canopus Observatory.
NR 36
TC 8
Z9 8
U1 0
U2 16
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 48
DI 10.1088/0004-637X/756/1/48
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300048
ER
PT J
AU Deheuvels, S
Garcia, RA
Chaplin, WJ
Basu, S
Antia, HM
Appourchaux, T
Benomar, O
Davies, GR
Elsworth, Y
Gizon, L
Goupil, MJ
Reese, DR
Regulo, C
Schou, J
Stahn, T
Casagrande, L
Christensen-Dalsgaard, J
Fischer, D
Hekker, S
Kjeldsen, H
Mathur, S
Mosser, B
Pinsonneault, M
Valenti, J
Christiansen, JL
Kinemuchi, K
Mullally, F
AF Deheuvels, S.
Garcia, R. A.
Chaplin, W. J.
Basu, S.
Antia, H. M.
Appourchaux, T.
Benomar, O.
Davies, G. R.
Elsworth, Y.
Gizon, L.
Goupil, M. J.
Reese, D. R.
Regulo, C.
Schou, J.
Stahn, T.
Casagrande, L.
Christensen-Dalsgaard, J.
Fischer, D.
Hekker, S.
Kjeldsen, H.
Mathur, S.
Mosser, B.
Pinsonneault, M.
Valenti, J.
Christiansen, J. L.
Kinemuchi, K.
Mullally, F.
TI SEISMIC EVIDENCE FOR A RAPIDLY ROTATING CORE IN A LOWER-GIANT-BRANCH
STAR OBSERVED WITH KEPLER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: evolution; stars: individual (KIC 7341231); stars: interiors;
stars: oscillations
ID SOLAR-LIKE OSCILLATIONS; LOW-MASS STARS; ANGULAR-MOMENTUM TRANSPORT;
PROPER-MOTION STARS; SUN-LIKE STAR; MAIN-SEQUENCE; MIXED-MODES; RED
GIANTS; DIFFERENTIAL ROTATION; HD 49385
AB Rotation is expected to have an important influence on the structure and the evolution of stars. However, the mechanisms of angular momentum transport in stars remain theoretically uncertain and very complex to take into account in stellar models. To achieve a better understanding of these processes, we desperately need observational constraints on the internal rotation of stars, which until very recently was restricted to the Sun. In this paper, we report the detection of mixed modes-i.e., modes that behave both as g modes in the core and as p modes in the envelope-in the spectrum of the early red giant KIC 7341231, which was observed during one year with the Kepler spacecraft. By performing an analysis of the oscillation spectrum of the star, we show that its non-radial modes are clearly split by stellar rotation and we are able to determine precisely the rotational splittings of 18 modes. We then find a stellar model that reproduces very well the observed atmospheric and seismic properties of the star. We use this model to perform inversions of the internal rotation profile of the star, which enables us to show that the core of the star is rotating at least five times faster than the envelope. This will shed new light on the processes of transport of angular momentum in stars. In particular, this result can be used to place constraints on the angular momentum coupling between the core and the envelope of early red giants, which could help us discriminate between the theories that have been proposed over the last few decades.
C1 [Deheuvels, S.; Basu, S.; Fischer, D.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Deheuvels, S.; Goupil, M. J.; Mosser, B.] Univ Paris 07, Univ Paris 06, Observ Paris, LESIA,UMR8109,CNRS, F-92195 Meudon, France.
[Deheuvels, S.; Garcia, R. A.; Chaplin, W. J.; Pinsonneault, M.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Garcia, R. A.; Davies, G. R.] Univ Paris Diderot, Lab AIM, CEA DSM, CNRS,CEA,IRFU,SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Chaplin, W. J.; Elsworth, Y.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Antia, H. M.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Appourchaux, T.] Univ Paris 11, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Benomar, O.] Univ Sydney, SIfA, Sch Phys, Sydney, NSW 2006, Australia.
[Gizon, L.; Stahn, T.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Gizon, L.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Reese, D. R.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Regulo, C.] Inst Astrofs Canarias, E-38205 Tenerife, Spain.
[Regulo, C.] Univ La Laguna, Dpto Astrofs, E-38206 Tenerife, Spain.
[Schou, J.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Casagrande, L.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia.
[Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, DASC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 HX Amsterdam, Netherlands.
[Mathur, S.] NCAR, High Altitude Observ, Boulder, CO 80307 USA.
[Pinsonneault, M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Valenti, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Christiansen, J. L.; Mullally, F.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kinemuchi, K.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Deheuvels, S (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA.
RI Gizon, Laurent/B-9457-2008;
OI Antia, H. M./0000-0001-7549-9684; Davies, Guy/0000-0002-4290-7351; Basu,
Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776;
Fischer, Debra/0000-0003-2221-0861
FU NASA's Science Mission Directorate; National Science Foundation of the
United States [NSF PHY0551164]; NSF [AST-1105930]; UK Science and
Technology Facilities Council (STFC); German Science Foundation [SFB
963]; University of Liege; Spanish National Research Plan
[AYA2010-17803]; Netherlands Organisation of Scientific Research (NWO);
National Science Foundation
FX The authors are very grateful to the Kepler team for building such a
marvelous mission and providing exquisite data for seismology. Funding
for this Discovery mission is provided by NASA's Science Mission
Directorate. We wish to thank the KITP at UCSB for their warm
hospitality during the research program "Asteroseismology in the Space
Age." This KITP program was supported in part by the National Science
Foundation of the United States under grant No. NSF PHY0551164. This
work was supported in part by NSF grant AST-1105930 (S. D. and S. B.).
W.J.C. and Y.E. acknowledge financial support from the UK Science and
Technology Facilities Council (STFC). L. G. and T. S. acknowledge
support from the German Science Foundation under SFB 963 Astrophysical
Flow Instabilities and Turbulence. D. R. R. acknowledges financial
support through a postdoctoral fellowship from the "Subside fdral pour
la recherche 2011," University of Liege. This research was partially
supported by grant AYA2010-17803 from the Spanish National Research Plan
(C. R.). S. H. acknowledges financial support from the Netherlands
Organisation of Scientific Research (NWO). NCAR is partially funded by
the National Science Foundation.
NR 115
TC 149
Z9 149
U1 2
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 19
DI 10.1088/0004-637X/756/1/19
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300019
ER
PT J
AU Greve, TR
Vieira, JD
Weiss, A
Aguirre, JE
Aird, KA
Ashby, MLN
Benson, BA
Bleem, LE
Bradford, CM
Brodwin, M
Carlstrom, JE
Chang, CL
Chapman, SC
Crawford, TM
de Breuck, C
de Haan, T
Dobbs, MA
Downes, T
Fassnacht, CD
Fazio, G
George, EM
Gladders, M
Gonzalez, AH
Halverson, NW
Hezaveh, Y
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Johnson, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Malkan, M
Marrone, DP
McIntyre, V
McMahon, JJ
Mehl, J
Menten, KM
Meyer, SS
Montroy, T
Murphy, EJ
Natoli, T
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Rosenman, M
Ruel, J
Ruhl, JE
Schaffer, KK
Sharon, K
Shaw, L
Shirokoff, E
Stalder, B
Stanford, SA
Staniszewski, Z
Stark, AA
Story, K
Vanderlinde, K
Walsh, W
Welikala, N
Williamson, R
AF Greve, T. R.
Vieira, J. D.
Weiss, A.
Aguirre, J. E.
Aird, K. A.
Ashby, M. L. N.
Benson, B. A.
Bleem, L. E.
Bradford, C. M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Chapman, S. C.
Crawford, T. M.
de Breuck, C.
de Haan, T.
Dobbs, M. A.
Downes, T.
Fassnacht, C. D.
Fazio, G.
George, E. M.
Gladders, M.
Gonzalez, A. H.
Halverson, N. W.
Hezaveh, Y.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Johnson, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Malkan, M.
Marrone, D. P.
McIntyre, V.
McMahon, J. J.
Mehl, J.
Menten, K. M.
Meyer, S. S.
Montroy, T.
Murphy, E. J.
Natoli, T.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Rosenman, M.
Ruel, J.
Ruhl, J. E.
Schaffer, K. K.
Sharon, K.
Shaw, L.
Shirokoff, E.
Stalder, B.
Stanford, S. A.
Staniszewski, Z.
Stark, A. A.
Story, K.
Vanderlinde, K.
Walsh, W.
Welikala, N.
Williamson, R.
TI SUBMILLIMETER OBSERVATIONS OF MILLIMETER BRIGHT GALAXIES DISCOVERED BY
THE SOUTH POLE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift;
galaxies: starburst; submillimeter: galaxies
ID SPECTRAL ENERGY-DISTRIBUTIONS; DEGREE EXTRAGALACTIC SURVEY; FAR-INFRARED
PROPERTIES; STAR-FORMATION RATE; MU-M OBSERVATIONS; HIGH-REDSHIFT;
HERSCHEL-ATLAS; BULLET CLUSTER; NUMBER COUNTS; MOLECULAR GAS
AB We present APEX SABOCA 350 mu m and LABOCA 870 mu m observations of 11 representative examples of the rare, extremely bright (S-1.4mm > 15 mJy), dust-dominated millimeter-selected galaxies recently discovered by the South Pole Telescope. All 11 sources are robustly detected with LABOCA with 40 mJy < S-870 mu m < 130 mJy, approximately an order of magnitude higher than the canonical submillimeter galaxy (SMG) population. Six of the sources are also detected by SABOCA at > 3 sigma, with the detections or upper limits providing a key constraint on the shape of the spectral energy distribution (SED) near its peak. We model the SEDs of these galaxies using a simple modified blackbody and perform the same analysis on samples of SMGs of known redshift from the literature. These calibration samples inform the distribution of dust temperature for similar SMG populations, and this dust temperature prior allows us to derive photometric redshift estimates and far-infrared luminosities for the sources. We find a median redshift of (z) over bar = 3.0, higher than the (z) over bar = 2.2 inferred for the normal SMG population. We also derive the apparent size of the sources from the temperature and apparent luminosity, finding them to appear larger than our unlensed calibration sample, which supports the idea that these sources are gravitationally magnified by massive structures along the line of sight.
C1 [Greve, T. R.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England.
[Vieira, J. D.; Downes, T.; Lueker, M.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA.
[Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Aguirre, J. E.; Rosenman, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Aird, K. A.; Carlstrom, J. E.; Crawford, T. M.; Gladders, M.; High, F. W.; Hrubes, J. D.; Leitch, E. M.; Luong-Van, D.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Ashby, M. L. N.; Brodwin, M.; Fazio, G.; Stalder, B.; Stark, A. A.; Walsh, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Gladders, M.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Sharon, K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; Meyer, S. S.; Natoli, T.; Pryke, C.; Story, K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bradford, C. M.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[de Breuck, C.] European So Observ, D-85748 Garching, Germany.
[de Haan, T.; Dobbs, M. A.; Hezaveh, Y.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Fassnacht, C. D.; Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Johnson, M.; Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Montroy, T.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA.
[Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Rest, A.; Ruel, J.; Stalder, B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Welikala, N.] CNRS, F-91405 Orsay, France.
RP Greve, TR (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
EM tgreve@star.ucl.ac.uk
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Marrone,
Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; De Breuck,
Carlos/0000-0002-6637-3315; Stark, Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics
Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore
Foundation; IDA; National Sciences and Engineering Research Council of
Canada; Canada Research Chairs program; Canadian Institute for Advanced
Research; Alfred P. Sloan Research Fellowship; Becker Fund of the
Smithsonian Institution; National Aeronautics and Space Administration
FX The authors thank A. Blain and N. Scoville for stimulating discussions
and guidance. We are grateful to the competent staff at the APEX base
camp in Sequitor, Chile. The South Pole Telescope is supported by the
National Science Foundation through grants ANT-0638937 and ANT-0130612.
Partial support is also provided by the NSF Physics Frontier Center
grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the
University of Chicago, the Kavli Foundation, and the Gordon and Betty
Moore Foundation. T. R. G. acknowledges support from IDA. The McGill
group acknowledges funding from the National Sciences and Engineering
Research Council of Canada, Canada Research Chairs program, and the
Canadian Institute for Advanced Research. M. D. acknowledges support
from an Alfred P. Sloan Research Fellowship. A. A. S. acknowledges
support by the Becker Fund of the Smithsonian Institution. This research
has made use of the NASA/IPAC Extragalactic Database (NED), which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. Finally, we are grateful to the directors of ESO and the
SMA for granting us director's discretionary time.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 101
DI 10.1088/0004-637X/756/1/101
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300101
ER
PT J
AU Haghighipour, N
Butler, RP
Rivera, EJ
Henry, GW
Vogt, SS
AF Haghighipour, Nader
Butler, R. Paul
Rivera, Eugenio J.
Henry, Gregory W.
Vogt, Steven S.
TI THE LICK-CARNEGIE SURVEY: A NEW TWO-PLANET SYSTEM AROUND THE STAR HD
207832
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HD 207832)
ID GENEVA-COPENHAGEN SURVEY; HOT-JUPITER SYSTEMS; CIRCLE-PLUS PLANET;
TERRESTRIAL PLANETS; SOLAR NEIGHBORHOOD; HABITABLE ZONE; F-DWARF;
PHOTOMETRY; SEARCH; EARTH
AB Keck/HIRES precision radial velocities of HD 207832 indicate the presence of two Jovian-type planetary companions in Keplerian orbits around this G star. The planets have minimum masses of M sin i = 0.56 M-Jup and 0.73 M-Jup, with orbital periods of similar to 162 and similar to 1156 days, and eccentricities of 0.13 and 0.27, respectively. Stromgren b and y photometry reveals a clear stellar rotation signature of the host star with a period of 17.8 days, well separated from the period of the radial velocity variations, reinforcing their Keplerian origin. The values of the semimajor axes of the planets suggest that these objects have migrated from the region of giant planet formation to closer orbits. In order to examine the possibility of the existence of additional (small) planets in the system, we studied the orbital stability of hypothetical terrestrial-sized objects in the region between the two planets and interior to the orbit of the inner body. Results indicated that stable orbits exist only in a small region interior to planet b. However, the current observational data offer no evidence for the existence of additional objects in this system.
C1 [Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Butler, R. Paul] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Rivera, Eugenio J.; Vogt, Steven S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Lick Observ, UCO, Santa Cruz, CA 95064 USA.
[Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
RP Haghighipour, N (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
RI Butler, Robert/B-1125-2009
FU NASA Astrobiology Institute at the Institute for Astronomy, University
of Hawaii [NNA09DA77]; NASA EXOB [NNX09AN05G]; NASA OSS [NNX07AR40G];
NASA Keck PI program; Carnegie Institution of Washington; NASA; NSF
[AST-0307493]; Tennessee State University; State of Tennessee through
its Centers of Excellence program; UC-Keck; NASA-Keck; UH/IFA Time
Assignment Committees
FX N.H. acknowledges support from the NASA Astrobiology Institute under
Cooperative Agreement NNA09DA77 at the Institute for Astronomy,
University of Hawaii, and NASA EXOB grant NNX09AN05G. R. P. B.
acknowledges support from NASA OSS Grant NNX07AR40G, the NASA Keck PI
program, and from the Carnegie Institution of Washington. G. W. H.
acknowledges support from NASA, NSF, Tennessee State University, and the
State of Tennessee through its Centers of Excellence program. S. S. V.
gratefully acknowledges support from NSF grant AST-0307493. The work
herein is based on observations obtained at the W. M. Keck Observatory,
which is operated jointly by the University of California and the
California Institute of Technology. We thank the UC-Keck, NASA-Keck, and
UH/IFA Time Assignment Committees for their support. This research has
made use of the SIMBAD database, operated at CDS, Strasbourg, France.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
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DI 10.1088/0004-637X/756/1/91
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300091
ER
PT J
AU Hosokawa, T
Omukai, K
Yorke, HW
AF Hosokawa, Takashi
Omukai, Kazuyuki
Yorke, Harold W.
TI RAPIDLY ACCRETING SUPERGIANT PROTOSTARS: EMBRYOS OF SUPERMASSIVE BLACK
HOLES?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; cosmology: theory; early universe; galaxies:
formation; stars: formation
ID MASSIVE PRIMORDIAL STARS; 1ST STARS; VIRIAL TEMPERATURES;
POPULATION-III; PROTOSTELLAR FEEDBACK; DIRECT COLLAPSE; DISK ACCRETION;
EARLY UNIVERSE; QUASI-STARS; HII-REGIONS
AB Direct collapse of supermassive stars (SMSs) is a possible pathway for generating supermassive black holes in the early universe. It is expected that an SMS could form via very rapidmass accretion with M-* similar to 0.1-1 M-circle dot yr(-1) during the gravitational collapse of an atomic-cooling primordial gas cloud. In this paper, we study how stars would evolve under such extreme rapid mass accretion, focusing on the early evolution until the stellar mass reaches 10(3) M-circle dot. To this end, we numerically calculate the detailed interior structure of accreting stars with primordial element abundances. Our results show that for accretion rates higher than 10(-2) M-circle dot yr(-1), stellar evolution is qualitatively different from that expected at lower rates. While accreting at these high rates, the star always has a radius exceeding 100 R-circle dot, which increases monotonically with the stellar mass. The mass-radius relation for stellar masses exceeding similar to 100 M-circle dot follows the same track with R-* proportional to M-*(1/2) in all cases with accretion rates greater than or similar to 10(-2) M-circle dot yr(-1); at a stellar mass of 10(3) M-circle dot, the radius is similar or equal to 7000 R-circle dot (similar or equal to 30 AU). With higher accretion rates, the onset of hydrogen burning is shifted toward higher stellar masses. In particular, for accretion rates exceeding M-* greater than or similar to 0.1 M-circle dot yr(-1), there is no significant hydrogen burning even after 10(3) M-circle dot have accreted onto the protostar. Such "supergiant" protostars have effective temperatures as low as T-eff similar or equal to 5000 K throughout their evolution and because they hardly emit ionizing photons, they do not create an H II region or significantly heat their immediate surroundings. Thus, radiative feedback is unable to hinder the growth of rapidly accreting stars to masses in excess of 10(3) M-circle dot as long as material is accreted at rates M-* greater than or similar to 10(-2) M-circle dot yr(-1).
C1 [Hosokawa, Takashi; Yorke, Harold W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hosokawa, Takashi; Omukai, Kazuyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan.
RP Hosokawa, T (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Takashi.Hosokawa@jpl.nasa.gov; omukai@tap.scphys.kyoto-u.ac.jp;
hosokwtk@gmail.com
FU Japan Society for the Promotion of Science; Ministry of Education,
Science and Culture of Japan [2168407, 21244021]; National Aeronautics
and Space Administration (NASA)
FX The authors thank Francesco Palla, Mitchell Begelman, Zoltan Haiman,
Milos Milosavljevic, Jarrett Johnson, Neal Turner, Rolf Kuiper, Kohei
Inayoshi, and Naoki Yoshida for fruitful discussions and comments. T. H.
appreciates the support by Fellowship of the Japan Society for the
Promotion of Science for Research Abroad. K.O. is supported by the
Grants-in-Aid by the Ministry of Education, Science and Culture of Japan
(2168407 and 21244021). Portions of this work were conducted at the Jet
Propulsion Laboratory, California Institute of Technology, operating
under a contract with the National Aeronautics and Space Administration
(NASA).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
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SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300093
ER
PT J
AU Jevtic, N
Stine, P
Nilsen, W
Schweitzer, JS
Jenkins, JM
Klaus, TC
Lie, J
McCauliff, S
AF Jevtic, Nada
Stine, Peter
Nilsen, Wayne
Schweitzer, J. S.
Jenkins, Jon M.
Klaus, Todd C.
Lie, Ji
McCauliff, Sean
TI STOCHASTIC BRIGHTNESS VARIATIONS IN THE CENTRAL STAR OF PLANETARY NEBULA
NGC 6826
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; planetary nebulae: individual (NGC 6826); stars:
variables: general; telescopes
ID SOLAR-LIKE OSCILLATIONS; SUBDWARF B STARS; TIME-SERIES; STRANGE
ATTRACTORS; COMPACT PULSATORS; KEPLER; EVOLUTION; CURVES
AB One year of continuous Kepler Space Telescope data for the central object of planetary nebula NGC 6826 (KIC 12071221) were analyzed. KIC 12071221 has long-cadence light curves with stochastic brightness variations and broadband power spectra. The exception is a one-month long period during which variability was detected with a period of 14.8 hr. In search of the origin of this periodicity and in an attempt to better understand the complex NGC 6826 system, long-cadence KIC 12071221 data were analyzed using nonlinear time seriesmethods. Nonlinear projective noise reduction from a phase-space dimension of six lowered the tail of the power spectra at the higher frequencies by factors of 38-133, an unexpected result for light curves with no obvious dominant frequencies. Even more notable is the identification of a structured distribution of trajectories, or coherence, in the reconstructed phase space for vectors spanning an interval of 1.5 hr. Organization weakens as the delay increases and is lost for phase-space vectors spanning times longer than 10 hr. This may be indicative of a binary object which shares a common envelope and/or pulsations but for a complete understanding one or both may have to be combined with wind structure. Thus, an estimate is made of the timescale of the response to what we propose is stochastic driving. This estimate of the timescale of the organized response is made by monitoring the loss of structure in the distribution of trajectories in phase space, a novel application of nonlinear methodology that may be used on data sampled with any sampling time.
C1 [Jevtic, Nada; Stine, Peter] Bloomsburg Univ Penn, Bloomsburg, PA 17815 USA.
[Jevtic, Nada; Schweitzer, J. S.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Nilsen, Wayne] Boston Univ, Sch Management, Boston, MA 02215 USA.
[Jenkins, Jon M.; Lie, Ji] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Klaus, Todd C.; McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Jevtic, N (reprint author), Bloomsburg Univ Penn, 400 E 2nd St, Bloomsburg, PA 17815 USA.
EM njevtic@bloomu.edu; pstine@bloomu.edu; wnilsen@bu.edu;
schweitz@phys.uconn.edu; jon.jenkins@nasa.gov; Todd.Klaus@nasa.gov;
jie.li-1@nasa.gov; Sean.D.McCauliff@nasa.gov
FU NASA's Science Mission Directorate
FX Funding for the Kepler Mission is provided by NASA's Science Mission
Directorate. We thank the entire Kepler team for the development and
operations of this outstanding mission.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
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DI 10.1088/0004-637X/756/1/9
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300009
ER
PT J
AU Katsuda, S
Tsunemi, H
Mori, K
Uchida, H
Petre, R
Yamada, S
Akamatsu, H
Konami, S
Tamagawa, T
AF Katsuda, Satoru
Tsunemi, Hiroshi
Mori, Koji
Uchida, Hiroyuki
Petre, Robert
Yamada, Shin'ya
Akamatsu, Hiroki
Konami, Saori
Tamagawa, Toru
TI HIGH-RESOLUTION X-RAY SPECTROSCOPY OF THE GALACTIC SUPERNOVA REMNANT
PUPPIS A WITH XMM-NEWTON/RGS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atomic processes; ISM: abundances; ISM: individual objects (Puppis A);
ISM: supernova remnants; X-rays: ISM
ID PHOTON IMAGING CAMERA; NEUTRAL HYDROGEN; LINE EMISSION; NOVA REMNANT;
SPECTRUM; SUZAKU; 1E-0102.2-7219; DIAGNOSTICS; DISCOVERY; COMETS
AB We present high-resolution X-ray spectra of cloud-shock interaction regions in the eastern and northern rims of the Galactic supernova remnant Puppis A, using the Reflection Grating Spectrometer on board the XMM-Newton satellite. A number of emission lines including K alpha triplets of He-like N, O, and Ne are clearly resolved for the first time. Intensity ratios of forbidden to resonance lines in the triplets are found to be higher than predictions by thermal emission models having plausible plasma parameters. The anomalous line ratios cannot be reproduced by effects of resonance scattering, recombination, or inner-shell ionization processes, but could be explained by charge-exchange emission that should arise at interfaces between the cold/warm clouds and the hot plasma. Our observations thus provide observational support for charge-exchange X-ray emission in supernova remnants.
C1 [Katsuda, Satoru; Yamada, Shin'ya; Konami, Saori; 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.
[Akamatsu, Hiroki] Tokyo Metropolitan Univ, Dept Phys, Hachioji, Tokyo 1920397, Japan.
[Konami, Saori] Tokyo Univ Sci, Dept Phys, Shinjuku Ku, Tokyo 1628601, Japan.
RP Katsuda, S (reprint author), RIKEN, Inst Phys & Chem Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.
FU Ministry of Education, Culture, Sports, Science, and Technology
[23000004]; Special Postdoctoral Researchers Program in RIKEN
FX We thank Professor H. Tanuma for fruitful discussions about the
laboratory experiments of CX X-ray emission. We also thank the referee
for numerous comments which improved the quality of the paper. 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).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 49
DI 10.1088/0004-637X/756/1/49
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300049
ER
PT J
AU Kim, S
Wardlow, JL
Cooray, A
Fleuren, S
Sutherland, W
Khostovan, AA
Auld, R
Baes, M
Bussmann, RS
Buttiglione, S
Cava, A
Clements, D
Dariush, A
De Zotti, G
Dunne, L
Dye, S
Eales, S
Fritz, J
Hopwood, R
Ibar, E
Ivison, R
Jarvis, M
Maddox, S
Michalowski, MJ
Pascale, E
Pohlen, M
Rigby, E
Scott, D
Smith, DJB
Temi, P
van der Werf, P
AF Kim, Sam
Wardlow, Julie L.
Cooray, Asantha
Fleuren, S.
Sutherland, W.
Khostovan, A. A.
Auld, R.
Baes, M.
Bussmann, R. S.
Buttiglione, S.
Cava, A.
Clements, D.
Dariush, A.
De Zotti, G.
Dunne, L.
Dye, S.
Eales, S.
Fritz, J.
Hopwood, R.
Ibar, E.
Ivison, R.
Jarvis, M.
Maddox, S.
Michalowski, M. J.
Pascale, E.
Pohlen, M.
Rigby, E.
Scott, D.
Smith, D. J. B.
Temi, P.
van der Werf, P.
TI SPITZER-IRAC IDENTIFICATION OF HERSCHEL-ATLAS SPIRE SOURCES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; galaxies: starburst; infrared: galaxies
ID DEEP-FIELD-SOUTH; DEGREE EXTRAGALACTIC SURVEY; SCIENCE DEMONSTRATION
PHASE; DIGITAL SKY SURVEY; REDSHIFT SUBMILLIMETER GALAXIES; SPECTRAL
ENERGY-DISTRIBUTIONS; NEAR-INFRARED COUNTERPARTS; STAR-FORMING GALAXIES;
ARRAY CAMERA IRAC; SCUBA SUPER-MAP
AB We use Spitzer-IRAC data to identify near-infrared counterparts to submillimeter galaxies detected with Herschel-SPIRE at 250 mu m in the Herschel Astrophysical Terahertz Large Area Survey. Using a likelihood ratio analysis we identify 146 reliable IRAC counterparts to 123 SPIRE sources out of the 159 in the survey area. We find that, compared to the field population, the SPIRE counterparts occupy a distinct region of the 3.6 and 4.5 mu m color-magnitude space, and we use this property to identify 23 further counterparts to 13 SPIRE sources. The IRAC identification rate of 86% is significantly higher than those that have been demonstrated with wide-field ground-based optical and near-IR imaging of Herschel fields. We estimate a false identification rate of 3.6%, corresponding to 4-5 sources. Among the 73 counterparts that are undetected in Sloan Digital Sky Survey, 57 have both 3.6 and 4.5 mu m coverage. Of these, 43 have [3.6]-[4.5] > 0, indicating that they are likely to be at z greater than or similar to 1.4. Thus, similar to 40% of identified SPIRE galaxies are likely to be high-redshift (z greater than or similar to 1.4) sources. We discuss the statistical properties of the IRAC-identified SPIRE galaxy sample including far-IR luminosities, dust temperatures, star formation rates, and stellar masses. The majority of our detected galaxies have 10(10)-10(11) L-circle dot total IR luminosities and are not intense starbursting galaxies as those found at z similar to 2, but they have a factor of 2-3 above average specific star formation rates compared to near-IR selected galaxy samples.
C1 [Kim, Sam; Wardlow, Julie L.; Cooray, Asantha; Khostovan, A. A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Fleuren, S.; Sutherland, W.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England.
[Auld, R.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Buttiglione, S.; De Zotti, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain.
[Clements, D.; Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[De Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Dunne, L.; Maddox, S.; Rigby, E.] Univ Canterbury, Dept Phys & Astron, Christchurch 8041, New Zealand.
[Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Ibar, E.; Ivison, R.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Jarvis, M.; Smith, D. J. B.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
[Michalowski, M. J.] Univ Edinburgh, Royal Observ, Scottish Univ Phys Alliance, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Kim, S (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
RI Baes, Maarten/I-6985-2013; Wardlow, Julie/C-9903-2015; Ivison,
R./G-4450-2011; Cava, Antonio/C-5274-2017;
OI Smith, Daniel/0000-0001-9708-253X; Baes, Maarten/0000-0002-3930-2757;
Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313;
Cava, Antonio/0000-0002-4821-1275; De Zotti,
Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X;
Scott, Douglas/0000-0002-6878-9840; Dye, Simon/0000-0002-1318-8343
FU NASA; JPL/Caltech; NASA Herschel Science Center; Alfred P. Sloan
Foundation; National Science Foundation; U.S. Department of Energy;
National Aeronautics and Space Administration; Japanese Monbukagakusho;
Max Planck Society; Higher Education Funding Council for England;
American Museum of Natural History; Astrophysical Institute Potsdam;
University of Basel; University of Cambridge; Case Western Reserve
University; University of Chicago; Drexel University; Fermilab;
Institute for Advanced Study; Japan Participation Group; Johns Hopkins
University; Joint Institute for Nuclear Astrophysics; Kavli Institute
for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese
Academy of Sciences (LAMOST); Los Alamos National Laboratory;
Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for
Astrophysics (MPA); New Mexico State University; Ohio State University;
University of Pittsburgh; University of Portsmouth; Princeton
University; United States Naval Observatory; University of Washington;
NSF CAREER [AST-0645427]; NASA [NNX10AD42G]; Caltech/JPL for US
participation in Herschel-ATLAS
FX Herschel-ATLAS is a project which uses Herschel, an ESA space
observatory with science instruments provided by European-led Principal
Investigator consortia and with important participation from NASA. The
H-ATLAS Web site is http://www.h-atlas.org/. This work 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. US participants in H-ATLAS also
acknowledge support from the NASA Herschel Science Center through a
contract from JPL/Caltech.; Funding for the SDSS and SDSS-II has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, the U.S. Department of
Energy, the National Aeronautics and Space Administration, the Japanese
Monbukagakusho, the Max Planck Society, and the Higher Education Funding
Council for England. The SDSS Web site is http://www.sdss.org/.; The
SDSS is managed by the Astrophysical Research Consortium for the
Participating Institutions. The Participating Institutions are the
American Museum of Natural History, Astrophysical Institute Potsdam,
University of Basel, University of Cambridge, Case Western Reserve
University, University of Chicago, Drexel University, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, Johns
Hopkins University, the Joint Institute for Nuclear Astrophysics, the
Kavli Institute for Particle Astrophysics and Cosmology, the Korean
Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, Ohio State University, University of Pittsburgh, University
of Portsmouth, Princeton University, the United States Naval
Observatory, and the University of Washington.; We thank Giulia
Rodighiero for providing us electronic tables of COSMOS and GOODS SED
fitting results. The UCI group acknowledges support from NSF CAREER
AST-0645427, NASA NNX10AD42G, and an award from Caltech/JPL for US
participation in Herschel-ATLAS.
NR 109
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 28
DI 10.1088/0004-637X/756/1/28
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300028
ER
PT J
AU Koay, JY
Macquart, JP
Rickett, BJ
Bignall, HE
Jauncey, DL
Pursimo, T
Reynolds, C
Lovell, JEJ
Kedziora-Chudczer, L
Ojha, R
AF Koay, J. Y.
Macquart, J. -P.
Rickett, B. J.
Bignall, H. E.
Jauncey, D. L.
Pursimo, T.
Reynolds, C.
Lovell, J. E. J.
Kedziora-Chudczer, L.
Ojha, R.
TI WHY DO COMPACT ACTIVE GALACTIC NUCLEI AT HIGH REDSHIFT SCINTILLATE LESS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: active; intergalactic medium; ISM:
structure; quasars: general; radio continuum: ISM
ID EXTRAGALACTIC RADIO-SOURCES; ALL-SKY SURVEY; INTERSTELLAR SCINTILLATION;
INDUCED VARIABILITY; BRIGHTNESS TEMPERATURE; INTRADAY VARIABILITY;
QUASAR J1819+3845; ANNUAL MODULATION; ANNUAL CYCLES; GALAXIES
AB The fraction of compact active galactic nuclei (AGNs) that exhibit interstellar scintillation (ISS) at radiowavelengths, as well as their scintillation amplitudes, have been found to decrease significantly for sources at redshifts z greater than or similar to 2. This can be attributed to an increase in the angular sizes of the mu as-scale cores or a decrease in the flux densities of the compact mu as cores relative to that of the mas-scale components with increasing redshift, possibly arising from (1) the space-time curvature of an expanding universe, (2) AGN evolution, (3) source selection biases, (4) scatter broadening in the ionized intergalactic medium (IGM) and intervening galaxies, or (5) gravitational lensing. We examine the frequency scaling of this redshift dependence of ISS to determine its origin, using data from a dual-frequency survey of ISS of 128 sources at 0 less than or similar to z less than or similar to 4. We present a novel method of analysis which accounts for selection effects in the source sample. We determine that the redshift dependence of ISS is partially linked to the steepening of source spectral indices (alpha(8.4)(4.9)) with redshift, caused either by selection biases or AGN evolution, coupled with weaker ISS in the alpha(8.4)(4.9) < -0.4 sources. Selecting only the -0.4 < alpha(8.4)(4.9) < 0.4 sources, we find that the redshift dependence of ISS is still significant, but is not significantly steeper than the expected (1+z)(0.5) scaling of source angular sizes due to cosmological expansion for a brightness temperature and flux-limited sample of sources. We find no significant evidence for scatter broadening in the IGM, ruling it out as the main cause of the redshift dependence of ISS. We obtain an upper limit to IGM scatter broadening of less than or similar to 110 mu as at 4.9 GHz with 99% confidence for all lines of sight and as low as less than or similar to 8 mu as for sight lines to the most compact, similar to 10 mu as sources.
C1 [Koay, J. Y.; Macquart, J. -P.; Bignall, H. E.; Reynolds, C.] Curtin Univ Technol, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Rickett, B. J.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA.
[Jauncey, D. L.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Jauncey, D. L.] Mt Stromlo & Siding Spring Observ, Weston, ACT 2611, Australia.
[Pursimo, T.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Spain.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Kedziora-Chudczer, L.] Univ New S Wales, Sch Phys & Astrophys, Sydney, NSW 2052, Australia.
[Ojha, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ojha, R.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
RP Koay, JY (reprint author), Curtin Univ Technol, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
EM kevin.koay@icrar.org
RI Macquart, Jean-Pierre/B-5306-2013; Reynolds, Cormac/B-5635-2013;
Bignall, Hayley/B-2867-2013; Koay, Jun Yi /E-4952-2015
OI Reynolds, Cormac/0000-0002-8978-0626; Bignall,
Hayley/0000-0001-6247-3071; Koay, Jun Yi /0000-0002-7029-6658
FU Curtin University; U.S. National Science Foundation (NSF) [AST
05-07713]; NASA Postdoctoral Program at the Goddard Space Flight Center;
NASA; NSF
FX J.Y.K. is supported by the Curtin Strategic International Research
Scholarship (CSIRS) provided by Curtin University. B.J.R. thanks the
U.S. National Science Foundation (NSF) for partial support under grant
AST 05-07713 and for the hospitality of the Cavendish Astrophysics group
at Cambridge University. R. O. 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 all thank the operators and scientific staff at the VLA;
in particular we thank Vivek Dhawan for his extensive advice and help
during our long sequence of observations. The VLA is part of the
National Radio Astronomy Observatory (NRAO), which is a facility of the
NSF operated under cooperative agreement by Associated Universities,
Inc. This study made use of data from the WHAM northern sky survey,
which is funded by the NSF. We used data obtained from the NASA/IPAC
Extragalactic Database (NED), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA, as well as the SIMBAD database, operated at CDS, Strasbourg,
France.
NR 67
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 29
DI 10.1088/0004-637X/756/1/29
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300029
ER
PT J
AU Li, D
Goldsmith, PF
AF Li, Di
Goldsmith, Paul F.
TI IS THE TAURUS B213 REGION A TRUE FILAMENT?: OBSERVATIONS OF MULTIPLE
CYANOACETYLENE TRANSITIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (Taurus); ISM: molecules; ISM: structure;
techniques: spectroscopic
ID DENSE CORE FORMATION; MOLECULAR CLOUD; STAR-FORMATION; HC3N;
FRAGMENTATION; SIMULATIONS; EVOLUTION; HERSCHEL; GAS; EXCITATION
AB We have obtained spectra of the J = 2-1 and 10-9 transitions of cyanoacetylene (HC3N) toward a collection of positions in the most prominent filament, B213, in the Taurus molecular cloud. The analysis of the excitation conditions of these transitions reveals an average gas H-2 volume density of (1.8 +/- 0.7) x10(4) cm(-3). Based on column density derived from the Two Micron All Sky Survey and this volume density, the line-of-sight dimension of the high-density portion of B213 is found to be similar or equal to 0.12 pc, which is comparable to the smaller projected dimension and much smaller than the elongated dimension of B213 (similar to 2.4 pc). B213 is thus likely a true cylinder-like filament rather than a sheet seen edge-on. The line width and velocity gradient seen in HC3N are also consistent with Taurus B213 being a self-gravitating filament in the early stage of either fragmentation and/or collapse.
C1 [Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Li, Di] Space Sci Inst, Boulder, CO USA.
[Li, Di; Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Li, D (reprint author), Chinese Acad Sci, Natl Astron Observ, Datun Rd A20, Beijing 100012, Peoples R China.
EM dili@nao.ac.cn
RI Goldsmith, Paul/H-3159-2016
FU China Ministry of Science and Technology [2012CB821800]; National
Aeronautics and Space Administration
FX This work has been partly supported by China Ministry of Science and
Technology under State Key Development Program for Basic Research
(2012CB821800). We thank the staff at the Green Bank Telescope and the
Arizona Radio Observatory for their support during these observations.
We also appreciate very helpful discussions with Steve Stahler on
molecular cloud evolution. We acknowledge valuable input from Hao Gong
and Pak-Shing Li regarding numerical simulations. We thank Laurent
Wiesenfeld for communicating his most recent calculations of
HC3N collisional excitation rates. This research was carried
out in part at the Jet Propulsion Laboratory, California Institute of
Technology which is supported by the National Aeronautics and Space
Administration.
NR 39
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 12
DI 10.1088/0004-637X/756/1/12
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300012
ER
PT J
AU Lin, L
Gogus, E
Baring, MG
Granot, J
Kouveliotou, C
Kaneko, Y
van der Horst, A
Gruber, D
von Kienlin, A
Younes, G
Watts, AL
Gehrels, N
AF Lin, Lin
Gogus, Ersin
Baring, Matthew G.
Granot, Jonathan
Kouveliotou, Chryssa
Kaneko, Yuki
van der Horst, Alexander
Gruber, David
von Kienlin, Andreas
Younes, George
Watts, Anna L.
Gehrels, Neil
TI BROADBAND SPECTRAL INVESTIGATIONS OF SGR J1550-5418 BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (SGR J1550-5418, 1E 1547.0-5408, PSR J1550-5418);
stars: neutron; X-rays: bursts
ID X-RAY PULSAR; SOFT GAMMA-REPEATERS; MAGNETIZED NEUTRON-STARS; 1E
1547.0-5408; RXTE OBSERVATIONS; 2009 OUTBURSTS; MONITOR; SGR-1900+14;
1E-1547.0-5408; MAGNETARS
AB We present the results of our broadband spectral analysis of 42 SGR J1550-5418 bursts simultaneously detected with the Swift/X-ray Telescope (XRT) and the Fermi/Gamma-ray Burst Monitor (GBM), during the 2009 January active episode of the source. The unique spectral and temporal capabilities of the XRT windowed timing mode have allowed us to extend the GBM spectral coverage for these events down to the X-ray domain (0.5-10 keV). Our earlier analysis of the GBM data found that the SGR J1550-5418 burst spectra were described equally well with either a Comptonized model or with two blackbody functions; the two models were statistically indistinguishable. Our new broadband (0.5-200 keV) spectral fits show that, on average, the burst spectra are better described with two blackbody functions than with the Comptonized model. Thus, our joint XRT-GBM analysis clearly shows for the first time that the SGR J1550-5418 burst spectra might naturally be expected to exhibit a more truly thermalized character, such as a two-blackbody or even a multi-blackbody signal. Using the Swift and RXTE timing ephemeris for SGR J1550-5418 we construct the distribution of the XRT burst counts with spin phase and find that it is not correlated with the persistent X-ray emission pulse phase from SGR J1550-5418. These results indicate that the burst emitting sites on the neutron star need not to be co-located with hot spots emitting the bulk of the persistent X-ray emission. Finally, we show that there is a significant pulse phase dependence of the XRT burst counts, likely demonstrating that the surface magnetic field of SGR J1550-5418 is not uniform over the emission zones, since it is anticipated that regions with stronger surface magnetic field could trigger bursts more efficiently.
C1 [Lin, Lin; Gogus, Ersin; Kaneko, Yuki] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
[Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Granot, Jonathan] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Granot, Jonathan] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Granot, Jonathan] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[van der Horst, Alexander; Watts, Anna L.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Gruber, David; von Kienlin, Andreas] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Younes, George] USRA, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lin, L (reprint author), Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
EM linlin@sabanciuniv.edu
FU Post-Doctoral Research Fellowship of the Turkish Academy of Science;
NASA [NNX10AC59A]; ERC advanced research grant "GRBs"; GBM/Magnetar Key
Project (NASA) [NNH07ZDA001-GLAST]; Netherlands Organization for
Scientific Research (NWO) Vidi Grant
FX L.L. is funded through the Post-Doctoral Research Fellowship of the
Turkish Academy of Science. M. G. B. acknowledges support from NASA
through grant NNX10AC59A. J.G. is supported by the ERC advanced research
grant "GRBs." C. K. is partially funded by the GBM/Magnetar Key Project
(NASA grant NNH07ZDA001-GLAST, PI: C. Kouveliotou). A. L. W.
acknowledges support from a Netherlands Organization for Scientific
Research (NWO) Vidi Grant.
NR 34
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 54
DI 10.1088/0004-637X/756/1/54
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300054
ER
PT J
AU Lyra, W
Mac Low, MM
AF Lyra, Wladimir
Mac Low, Mordecai-Mark
TI ROSSBY WAVE INSTABILITY AT DEAD ZONE BOUNDARIES IN THREE-DIMENSIONAL
RESISTIVE MAGNETOHYDRODYNAMICAL GLOBAL MODELS OF PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; instabilities; magnetohydrodynamics (MHD);
methods: numerical; planets and satellites: formation; protoplanetary
disks
ID SPIRAL DENSITY WAVES; DIFFERENTIALLY ROTATING-DISKS; THIN ACCRETION
DISKS; PLANETESIMAL FORMATION; MAGNETOROTATIONAL-INSTABILITY;
CIRCUMSTELLAR DISKS; KEPLERIAN FLOW; BAROCLINIC INSTABILITY; TURBULENT
FLUCTUATIONS; STREAMING INSTABILITY
AB It has been suggested that the transition between magnetorotationally active and dead zones in protoplanetary disks should be prone to the excitation of vortices via Rossby wave instability (RWI). However, the only numerical evidence for this has come from alpha disk models, where the magnetic field evolution is not followed, and the effect of turbulence is parameterized by Laplacian viscosity. We aim to establish the phenomenology of the flow in the transition in three-dimensional resistive-magnetohydrodynamical models. We model the transition by a sharp jump in resistivity, as expected in the inner dead zone boundary, using the Pencil Code to simulate the flow. We find that vortices are readily excited in the dead side of the transition. We measure the mass accretion rate finding similar levels of Reynolds stress at the dead and active zones, at the alpha approximate to 10(-2) level. The vortex sits in a pressure maximum and does not migrate, surviving until the end of the simulation. A pressure maximum in the active zone also triggers the RWI. The magnetized vortex that results should be disrupted by parasitical magneto-elliptic instabilities, yet it subsists in high resolution. This suggests that either the parasitic modes are still numerically damped or that the RWI supplies vorticity faster than they can destroy it. We conclude that the resistive transition between the active and dead zones in the inner regions of protoplanetary disks, if sharp enough, can indeed excite vortices via RWI. Our results lend credence to previous works that relied on the alpha-disk approximation, and caution against the use of overly reduced azimuthal coverage on modeling this transition.
C1 [Lyra, Wladimir] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lyra, Wladimir; Mac Low, Mordecai-Mark] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
EM wlyra@jpl.nasa.gov; mordecai@amnh.org
OI Mac Low, Mordecai-Mark/0000-0003-0064-4060
FU National Science Foundation [AST10-09802, OCI-105357]; National
Aeronautics and Space Administration
FX The writing of this paper was started at the American Museum of Natural
History with financial support by the National Science Foundation under
grant No. AST10-09802, and completed at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. This work was performed under
allocation TG-MCA99S024 from the Extreme Science and Engineering
Discovery Environment (XSEDE), which is supported by National Science
Foundation grant No. OCI-105357. The computations were performed on the
Kraken system at the National Institute for Computational Sciences. We
thank the anonymous referee for useful suggestions.
NR 96
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 62
DI 10.1088/0004-637X/756/1/62
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300062
ER
PT J
AU Mirocha, J
Skory, S
Burns, JO
Wise, JH
AF Mirocha, Jordan
Skory, Stephen
Burns, Jack O.
Wise, John H.
TI OPTIMIZED MULTI-FREQUENCY SPECTRA FOR APPLICATIONS IN RADIATIVE FEEDBACK
AND COSMOLOGICAL REIONIZATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark ages, reionization, first stars; methods: numerical; radiative
transfer
ID MESH REFINEMENT SIMULATIONS; INTERGALACTIC MEDIUM; EDDINGTON TENSOR;
TRANSFER SCHEME; 1ST GALAXIES; BLACK-HOLES; X-RAYS; IONIZATION;
UNIVERSE; STARS
AB The recent implementation of radiative transfer algorithms in numerous hydrodynamics codes has led to a dramatic improvement in studies of feedback in various astrophysical environments. However, because of methodological limitations and computational expense, the spectra of radiation sources are generally sampled at only a few evenly spaced discrete emission frequencies. Using one-dimensional radiative transfer calculations, we investigate the discrepancies in gas properties surrounding model stars and accreting black holes that arise solely due to spectral discretization. We find that even in the idealized case of a static and uniform density field, commonly used discretization schemes induce errors in the neutral fraction and temperature by factors of two to three on average, and by over an order of magnitude in certain column density regimes. The consequences are most severe for radiative feedback operating on large scales, dense clumps of gas, and media consisting of multiple chemical species. We have developed a method for optimally constructing discrete spectra, and show that for two test cases of interest, carefully chosen four-bin spectra can eliminate errors associated with frequency resolution to high precision. Applying these findings to a fully three-dimensional radiation-hydrodynamic simulation of the early universe, we find that the H II region around a primordial star is substantially altered in both size and morphology, corroborating the one-dimensional prediction that discrete spectral energy distributions can lead to sizable inaccuracies in the physical properties of a medium, and as a result, the subsequent evolution and observable signatures of objects embedded within it.
C1 [Mirocha, Jordan; Skory, Stephen; Burns, Jack O.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Mirocha, Jordan; Skory, Stephen; Burns, Jack O.] NASA, Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA.
[Wise, John H.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
RP Mirocha, J (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Campus Box 389, Boulder, CO 80309 USA.
EM jordan.mirocha@colorado.edu
FU NASA Lunar Science Institute [NNA09DB30A]; National Science Foundation
[CNS-0821794]; University of Colorado Boulder
FX The authors thank Steven Furlanetto and Daniel Reynolds for feedback on
earlier versions of this draft, as well as the anonymous referee for a
thorough review and many helpful suggestions. The LUNAR consortium
(http://lunar.colorado.edu), headquartered at the University of
Colorado, is funded by the NASA Lunar Science Institute (via Cooperative
Agreement NNA09DB30A) to investigate concepts for astrophysical
observatories on the Moon. This work used the JANUS supercomputer, which
is supported by the National Science Foundation (award number
CNS-0821794) and the University of Colorado Boulder. The JANUS
supercomputer is a joint effort of the University of Colorado Boulder,
the University of Colorado Denver, and the National Center for
Atmospheric Research.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
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DI 10.1088/0004-637X/756/1/94
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300094
ER
PT J
AU Smith, MWL
Eales, SA
Gomez, HL
Roman-Duval, J
Fritz, J
Braun, R
Baes, M
Bendo, GJ
Blommaert, JADL
Boquien, M
Boselli, A
Clements, DL
Cooray, AR
Cortese, L
de Looze, I
Ford, GP
Gear, WK
Gentile, G
Gordon, KD
Kirk, J
Lebouteiller, V
Madden, S
Mentuch, E
O'Halloran, B
Page, MJ
Schulz, B
Spinoglio, L
Verstappen, J
Wilson, CD
Thilker, DA
AF Smith, M. W. L.
Eales, S. A.
Gomez, H. L.
Roman-Duval, J.
Fritz, J.
Braun, R.
Baes, M.
Bendo, G. J.
Blommaert, J. A. D. L.
Boquien, M.
Boselli, A.
Clements, D. L.
Cooray, A. R.
Cortese, L.
de Looze, I.
Ford, G. P.
Gear, W. K.
Gentile, G.
Gordon, K. D.
Kirk, J.
Lebouteiller, V.
Madden, S.
Mentuch, E.
O'Halloran, B.
Page, M. J.
Schulz, B.
Spinoglio, L.
Verstappen, J.
Wilson, C. D.
Thilker, D. A.
TI THE HERSCHEL EXPLOITATION OF LOCAL GALAXY ANDROMEDA (HELGA). II. DUST
AND GAS IN ANDROMEDA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: individual (M31); galaxies: ISM; Local
Group
ID MULTIBAND IMAGING PHOTOMETER; CO-TO-H-2 CONVERSION FACTOR; GAMMA-RAY
EMISSION; STAR-FORMATION; SPIRAL GALAXIES; MOLECULAR GAS;
INFRARED-EMISSION; SPECTRAL INDEX; GALACTIC PLANE; VIRGO CLUSTER
AB We present an analysis of the dust and gas in Andromeda, using Herschel images sampling the entire far-infrared peak. We fit a modified-blackbody model to similar to 4000 quasi-independent pixels with spatial resolution of similar to 140 pc and find that a variable dust-emissivity index (beta) is required to fit the data. We find no significant long-wavelength excess above this model, suggesting there is no cold dust component. We show that the gas-to-dust ratio varies radially, increasing from similar to 20 in the center to similar to 70 in the star-forming ring at 10 kpc, consistent with the metallicity gradient. In the 10 kpc ring the average beta is similar to 1.9, in good agreement with values determined for the Milky Way (MW). However, in contrast to the MW, we find significant radial variations in beta, which increases from 1.9 at 10 kpc to similar to 2.5 at a radius of 3.1 kpc and then decreases to 1.7 in the center. The dust temperature is fairly constant in the 10 kpc ring (ranging from 17 to 20 K), but increases strongly in the bulge to similar to 30 K. Within 3.1 kpc we find the dust temperature is highly correlated with the 3.6 mu m flux, suggesting the general stellar population in the bulge is the dominant source of dust heating there. At larger radii, there is a weak correlation between the star formation rate and dust temperature. We find no evidence for "dark gas" in M31 in contrast to recent results for the MW. Finally, we obtained an estimate of the CO X-factor by minimizing the dispersion in the gas-to-dust ratio, obtaining a value of (1.9 +/- 0.4) x 10(20) cm(-2) [K km s(-1)](-1).
C1 [Smith, M. W. L.; Eales, S. A.; Gomez, H. L.; Ford, G. P.; Gear, W. K.; Kirk, J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Roman-Duval, J.; Gordon, K. D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Fritz, J.; Baes, M.; de Looze, I.; Gentile, G.; Gordon, K. D.; Verstappen, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Braun, R.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Bendo, G. J.] Univ Manchester, UK ALMA Reg Ctr Node, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Blommaert, J. A. D. L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Boquien, M.; Boselli, A.] Univ Aix Marseille, Lab Astrophys Marseille LAM, F-13388 Marseille 13, France.
[Boquien, M.; Boselli, A.] CNRS, UMR7326, F-13388 Marseille 13, France.
[Clements, D. L.; O'Halloran, B.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Cooray, A. R.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA.
[Cooray, A. R.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Cortese, L.] European So Observ, D-85748 Garching, Germany.
[Lebouteiller, V.; Madden, S.] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France.
[Mentuch, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Schulz, B.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA.
[Spinoglio, L.] INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Wilson, C. D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
[Thilker, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Smith, MWL (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
EM Matthew.Smith@astro.cf.ac.uk
RI Baes, Maarten/I-6985-2013; Boquien, Mederic/J-5964-2015;
OI Baes, Maarten/0000-0002-3930-2757; Boquien, Mederic/0000-0003-0946-6176;
Lebouteiller, Vianney/0000-0002-7716-6223; Spinoglio,
Luigi/0000-0001-8840-1551; Cortese, Luca/0000-0002-7422-9823
FU BMVIT (Austria); A-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA;
CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC;
UKSA (UK); NASA (USA); European Community [229517]
FX We thank everyone involved with the Herschel Observatory. 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);
and IAC (Spain). This development has been supported by the funding
agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR
(Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).; SPIRE has been
developed by a consortium of institutes led by Cardiff University (UK)
and including: the 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, and the 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).;
The research leading to these results has received funding from the
European Community's Seventh Framework Programme (/FP7/2007-2013/) under
grant agreement No. 229517.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
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DI 10.1088/0004-637X/756/1/40
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300040
ER
PT J
AU Wu, JW
Tsai, CW
Sayers, J
Benford, D
Bridge, C
Blain, A
Eisenhardt, PRM
Stern, D
Petty, S
Assef, R
Bussmann, S
Comerford, JM
Cutri, R
Evans, NJ
Griffith, R
Jarrett, T
Lake, S
Lonsdale, C
Rho, J
Stanford, SA
Weiner, B
Wright, EL
Yan, L
AF Wu, Jingwen
Tsai, Chao-Wei
Sayers, Jack
Benford, Dominic
Bridge, Carrie
Blain, Andrew
Eisenhardt, Peter R. M.
Stern, Daniel
Petty, Sara
Assef, Roberto
Bussmann, Shane
Comerford, Julia M.
Cutri, Roc
Evans, Neal J., II
Griffith, Roger
Jarrett, Thomas
Lake, Sean
Lonsdale, Carol
Rho, Jeonghee
Stanford, S. Adam
Weiner, Benjamin
Wright, Edward L.
Yan, Lin
TI SUBMILLIMETER FOLLOW-UP OF WISE-SELECTED HYPERLUMINOUS GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: formation; galaxies: high-redshift; galaxies: ISM; galaxies:
starburst; infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; DUST-OBSCURED GALAXIES; STAR-FORMATION HISTORY;
INFRARED LUMINOUS GALAXIES; SPITZER MIDINFRARED SPECTROSCOPY; POLYCYCLIC
AROMATIC-HYDROCARBON; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE
BLACK-HOLES; DIGITAL SKY SURVEY; MU-M OBSERVATIONS
AB We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare (similar to 1000 all-sky) population of galaxies at high redshift (peaks at z = 2-3), which are faint or undetected by WISE at 3.4 and 4.6 mu m, yet are clearly detected at 12 and 22 mu m. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350-850 mu m, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 mu m, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature. We estimate their dust temperatures to be 60-120 K using a single-temperature model. Their infrared luminosities are well over 10(13) L-circle dot. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe. We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data.
C1 [Wu, Jingwen; Eisenhardt, Peter R. M.; Stern, Daniel; Assef, Roberto] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tsai, Chao-Wei; Cutri, Roc; Griffith, Roger; Jarrett, Thomas; Yan, Lin] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Sayers, Jack; Bridge, Carrie] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Benford, Dominic] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blain, Andrew] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Petty, Sara; Lake, Sean; Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Bussmann, Shane] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Comerford, Julia M.; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78731 USA.
[Lonsdale, Carol] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Rho, Jeonghee] SETI Inst, Mountain View, CA 94043 USA.
[Rho, Jeonghee] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Stanford, S. Adam] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Weiner, Benjamin] Steward Observ, Tucson, AZ 85721 USA.
RP Wu, JW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jingwen.wu@jpl.nasa.gov
RI Benford, Dominic/D-4760-2012;
OI Benford, Dominic/0000-0002-9884-4206; Weiner,
Benjamin/0000-0001-6065-7483
FU NASA; NSF [AST-1109116]; National Aeronautics and Space Administration;
National Science Foundation [AST 90-15755]; W. M. Keck Foundation;
Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science
FX J.W. and R. A. were 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. N.E. acknowledges
support from NSF Grant AST-1109116. This publication makes use of data
products from the Wide-field Infrared Survey Explorer, which is a joint
project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration. This work is based on
observations made with the Caltech Submillimeter Observatory, which is
operated by the California Institute of Technology under funding from
the National Science Foundation, contract AST 90-15755. This work uses
data obtained from the Spitzer Space Telescope, which is operated by the
Jet Propulsion Laboratory, California Institute of Technology under
contract with NASA. Some of the data presented herein were obtained at
the W. M. Keck Observatory, which is operated as a scientific
partnership among Caltech, the University of California, and NASA. The
Keck Observatory was made possible by the generous financial support of
the W. M. Keck Foundation. Some data reported here were obtained at the
MMT Observatory, a joint facility of the University of Arizona and the
Smithsonian Institution. This paper uses data from SDSS (DR 8). 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/.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
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AR 96
DI 10.1088/0004-637X/756/1/96
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300096
ER
PT J
AU Wu, YF
Liu, T
Meng, FY
Li, D
Qin, SL
Ju, BG
AF Wu, Yuefang
Liu, Tie
Meng, Fanyi
Li, Di
Qin, Sheng-Li
Ju, Bing-Gang
TI GAS EMISSIONS IN PLANCK COLD DUST CLUMPS-A SURVEY OF THE J=1-0
TRANSITIONS OF (CO)-C-12, (CO)-C-13, AND (CO)-O-18
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: clouds; ISM: kinematics and dynamics; ISM:
structure; stars: formation; stars: protostars
ID YOUNG STELLAR OBJECTS; INFRARED DARK CLOUDS; MASS PROTOSTELLAR
CANDIDATES; MOLECULAR CLOUDS; STAR-FORMATION; DENSE CORES; GALACTIC
PLANE; AMMONIA CORES; MILKY-WAY; NGC 1333
AB A survey toward 674 Planck cold clumps of the Early Cold Core Catalogue (ECC) in the J = 1-0 transitions of (CO)-C-12, (CO)-C-13, and (CO)-O-18 has been carried out using the Purple Mountain Observatory 13.7 m telescope. Six hundred seventy-three clumps were detected with (CO)-C-12 and (CO)-C-13 emission, and 68% of the sample has (CO)-O-18 emission. Additional velocity components were also identified. A close consistency of the three line peak velocities was revealed for the first time. Kinematic distances are given for all the velocity components, and half of the clumps are located within 0.5 and 1.5 kpc. Excitation temperatures range from 4 to 27 K, slightly larger than those of T-d. Line width analysis shows that the majority of ECC clumps are low-mass clumps. Column densities N-H2 span from 10(20) to 4.5 x 10(22) cm(-2) with an average value of (4.4 +/- 3.6) x 10(21) cm(-2). N-H2 cumulative fraction distribution deviates from the lognormal distribution, which is attributed to optical depth. The average abundance ratio of the (CO)-C-13 to (CO)-O-18 in these clumps is 7.0 +/- 3.8, higher than the terrestrial value. Dust and gas are well coupled in 95% of the clumps. Blue profile asymmetry, red profile asymmetry, and total line asymmetry were found in less than 10% of the clumps, generally indicating that star formation is not yet developed. Ten clumps were mapped. Twelve velocity components and 22 cores were obtained. Their morphologies include extended diffuse, dense, isolated, cometary, and filament, of which the last is the majority. Twenty cores are starless, and only seven cores seem to be in a gravitationally bound state. Planck cold clumps are the most quiescent among the samples of weak red IRAS, infrared dark clouds, UC H II candidates, extended green objects, and methanol maser sources, suggesting that Planck cold clumps have expanded the horizon of cold astronomy.
C1 [Wu, Yuefang; Liu, Tie] Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
[Meng, Fanyi] Peking Univ, Yuan Pei Sch, Beijing 100871, Peoples R China.
[Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China.
[Li, Di] Space Sci Inst, Boulder, CO USA.
[Li, Di] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Qin, Sheng-Li] Univ Cologne, Inst Phys, D-50937 Cologne, Germany.
[Ju, Bing-Gang] Purple Mt Observ, Qinghai Stn, Delingha 817000, Peoples R China.
[Ju, Bing-Gang] Chinese Acad Sci, Key Lab Radio Astron, Beijing, Peoples R China.
RP Wu, YF (reprint author), Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
EM ywu@pku.edu.cn
FU China Ministry of Science and Technology [2012CB821800]
FX We are grateful to the staff at the Qinghai Station of PMO for their
assistance during the observations. We thank the Key Laboratory for
Radio Astronomy, CAS, for partial support in the operation of the
telescope. This work was supported by China Ministry of Science and
Technology under State Key Development Program for Basic Research
(2012CB821800).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
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AR 76
DI 10.1088/0004-637X/756/1/76
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300076
ER
PT J
AU Zahn, O
Reichardt, CL
Shaw, L
Lidz, A
Aird, KA
Benson, BA
Bleem, LE
Carlstrom, JE
Chang, CL
Cho, HM
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Dore, O
Dudley, J
George, EM
Halverson, NW
Holder, GP
Holzapfel, WL
Hoover, S
Hou, Z
Hrubes, JD
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
McMahon, JJ
Mehl, J
Meyer, SS
Millea, M
Mohr, JJ
Montroy, TE
Natoli, T
Padin, S
Plagge, T
Pryke, C
Ruhl, JE
Schaffer, KK
Shirokoff, E
Spieler, HG
Staniszewski, Z
Stark, AA
Story, K
van Engelen, A
Vanderlinde, K
Vieira, JD
Williamson, R
AF Zahn, O.
Reichardt, C. L.
Shaw, L.
Lidz, A.
Aird, K. A.
Benson, B. A.
Bleem, L. E.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Dore, O.
Dudley, J.
George, E. M.
Halverson, N. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hou, Z.
Hrubes, J. D.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Millea, M.
Mohr, J. J.
Montroy, T. E.
Natoli, T.
Padin, S.
Plagge, T.
Pryke, C.
Ruhl, J. E.
Schaffer, K. K.
Shirokoff, E.
Spieler, H. G.
Staniszewski, Z.
Stark, A. A.
Story, K.
van Engelen, A.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
TI COSMIC MICROWAVE BACKGROUND CONSTRAINTS ON THE DURATION AND TIMING OF
REIONIZATION FROM THE SOUTH POLE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: theory; intergalactic medium; large-scale structure of
universe
ID LY-ALPHA EMITTERS; PROBE WMAP OBSERVATIONS; RADIATIVE-TRANSFER
SIMULATIONS; ZELDOVICH POWER SPECTRUM; HYDROGEN REIONIZATION; PATCHY
REIONIZATION; INTERGALACTIC MEDIUM; NEUTRAL HYDROGEN; BUBBLE-GROWTH;
HII-REGIONS
AB The epoch of reionization is a milestone of cosmological structure formation, marking the birth of the first objects massive enough to yield large numbers of ionizing photons. However, the mechanism and timescale of reionization remain largely unknown. Measurements of the cosmic microwave background (CMB) Doppler effect from ionizing bubbles embedded in large-scale velocity streams-known as the patchy kinetic Sunyaev-Zel'dovich (kSZ) effect-can be used to constrain the duration of reionization. When combined with large-scale CMB polarization measurements, the evolution of the ionized fraction, (x) over bar (e), can be inferred. Using new multi-frequency data from the South Pole Telescope (SPT), we show that the ionized fraction evolved relatively rapidly. For our basic foreground model, we find the kSZ power sourced by reionization at l = 3000 to be D-3000(patchy) <= 2.1 mu K-2 at 95% confidence. Using reionization simulations, we translate this to a limit on the duration of reionization of Delta z equivalent to z((x) over bare-0.20) - z((x) over bare-0.99) <= 4.4 (95% confidence). We find that this constraint depends on assumptions about the angular correlation between the thermal SZ power and the cosmic infrared background (CIB). Introducing the degree of correlation as a free parameter, we find that the limit on kSZ power weakens to D-3000(patchy) <= 4.9 mu K-2, implying Delta z <= 7.9 (95% confidence). We combine the SPT constraint on the duration of reionization with the Wilkinson Microwave Anisotropy Probe measurement of the integrated optical depth to probe the cosmic ionization history. We find that reionization ended with 95% confidence at z > 7.2 under the assumption of no tSZ-CIB correlation, and z > 5.8 when correlations are allowed. Improved constraints from the full SPT data set in conjunction with upcoming Herschel and Planck data should detect extended reionization at >95% confidence provided Delta z >= 2. These CMB observations complement other observational probes of the epoch of reionization such as the redshifted 21 cm line and narrowband surveys for Ly alpha-emitting galaxies.
C1 [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Shaw, L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Lidz, A.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Dore, O.; Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Joy, M.] NASA, Dept Space Sci, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Pryke, C.; Staniszewski, Z.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Zahn, O (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
EM zahn@berkeley.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; Stark,
Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics
Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore
Foundation; Berkeley Center for Cosmological Physics fellowship;
National Sciences and Engineering Research Council of Canada; Canada
Research Chairs program; Canadian Institute for Advanced Research; NASA
Hubble Fellowship [HF-51275.01]; KICP Fellowship; Alfred P. Sloan
Research Fellowship; Yale University; NSF [AST-1009811, 0709498]; Office
of Science of the U.S. Department of Energy [DE-AC02-05CH11231]
FX We thank Matt George, Guilaine Lagache, Cien Shang, David Spergel, Marco
Viero, and Matias Zaldarriaga for useful discussions. The South Pole
Telescope is supported by the National Science Foundation through grants
ANT-0638937 and ANT-0130612. Partial support is also provided by the NSF
Physics Frontier Center grant PHY-0114422 to the Kavli Institute of
Cosmological Physics at the University of Chicago, the Kavli Foundation
and the Gordon and Betty Moore Foundation. O. Zahn acknowledges support
from a Berkeley Center for Cosmological Physics fellowship. The McGill
group acknowledges funding from the National Sciences and Engineering
Research Council of Canada, Canada Research Chairs program, and the
Canadian Institute for Advanced Research. R. Keisler acknowledges
support from NASA Hubble Fellowship grant HF-51275.01. B. A. Benson is
supported by a KICP Fellowship. M. Dobbs acknowledges support from an
Alfred P. Sloan Research Fellowship. L. Shaw acknowledges the support of
Yale University and NSF grant AST-1009811. M. Millea and L. Knox
acknowledge the support of NSF grant 0709498. This research used
resources of the National Energy Research Scientific Computing Center,
which is supported by the Office of Science of the U. S. Department of
Energy under Contract No. DE-AC02-05CH11231. Some of the results in this
paper have been derived using the HEALPix package (Gorski et al. 2005).
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. We also acknowledge usage of the FFTW and
TeXShop software packages.
NR 111
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 65
DI 10.1088/0004-637X/756/1/65
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300065
ER
PT J
AU Zank, GP
Jetha, N
Hu, Q
Hunana, P
AF Zank, G. P.
Jetha, N.
Hu, Q.
Hunana, P.
TI THE TRANSPORT OF DENSITY FLUCTUATIONS THROUGHOUT THE HELIOSPHERE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); scattering; solar wind; Sun: heliosphere;
turbulence; waves
ID LOCAL INTERSTELLAR-MEDIUM; SOLAR-WIND; OUTER HELIOSPHERE;
MAGNETOHYDRODYNAMIC TURBULENCE; RADIO EMISSIONS; POWER SPECTRUM;
EVOLUTION; WAVES; INTERPLANETARY; SCATTERING
AB The solar wind is recognized as a turbulent magnetofluid, for which the properties of the turbulent velocity and magnetic field fluctuations are often described by the equations of incompressible magnetohydrodynamics (MHD). However, low-frequency density turbulence is also ubiquitous. On the basis of a nearly incompressible formulation of MHD in the expanding inhomogeneous solar wind, we derive the transport equation for the variance of the density fluctuations . The transport equation shows that density fluctuations behave as a passive scalar in the supersonic solar wind. In the absence of sources of density turbulence, such as within 1AU, the variance similar to r(-4). In the outer heliosphere beyond 1 AU, the shear between fast and slow streams, the propagation of shocks, and the creation of interstellar pickup ions all act as sources of density turbulence. The model density fluctuation variance evolves with heliocentric distance within similar to 30 AU as similar to r(-3.3) after which it flattens and then slowly increases. This is precisely the radial profile for the density fluctuation variance observed by Voyager 2. Using a different analysis technique, we confirm the radial profile for of Bellamy, Cairns, & Smith using Voyager 2 data. We conclude that a passive scalar description for density fluctuations in the supersonic solar wind can explain the density fluctuation variance observed in both the inner and the outer heliosphere.
C1 [Zank, G. P.; Jetha, N.; Hu, Q.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Zank, G. P.; Hu, Q.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Hunana, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zank, GP (reprint author), Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
EM garyp.zank@gmail.com
FU NASA [NNX08AJ33G, 37102-2, NNX09AG70G, NNX09AG63G, NNX09AJ79G,
NNG05EC85C, A991132BT, NNX09AP74A, NNX10AE46G, NNX09AW45G]; NSF
[ATM-0904007]; NASA Postdoctoral Program
FX We acknowledge the partial support of NASA grants NNX08AJ33G, Subaward
37102-2, NNX09AG70G, NNX09AG63G, NNX09AJ79G, NNG05EC85C, Subcontract
A991132BT, NNX09AP74A, NNX10AE46G, NNX09AW45G, and NSF grant
ATM-0904007. P. H. was supported by the NASA Postdoctoral Program, which
is administered by ORAU. We thank Professor Iver Cairns for generously
providing the data used in the top panel of Figure 2. G.P.Z. thanks Iver
Cairns, John Armstrong, and Steve Spangler for useful discussions.
NR 33
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 21
DI 10.1088/0004-637X/756/1/21
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300021
ER
PT J
AU Zheng, WK
Akerlof, CW
Pandey, SB
Mckay, TA
Zhang, BB
Zhang, B
Sakamoto, T
AF Zheng, WeiKang
Akerlof, Carl W.
Pandey, Shashi B.
McKay, Timothy A.
Zhang, BinBin
Zhang, Bing
Sakamoto, Takanori
TI GRB 110709A, 111117A, AND 120107A: FAINT HIGH-ENERGY GAMMA-RAY PHOTON
EMISSION FROM FERMI-LAT OBSERVATIONS AND DEMOGRAPHIC IMPLICATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 110709A, GRB 111117A, GRB 120107A)
ID LARGE-AREA TELESCOPE; BURST; MISSION; DETECTOR; NEEDLES
AB Launched on 2008 June 11, the Large Area Telescope (LAT) instrument on board the Fermi Gamma-ray Space Telescope has provided a rare opportunity to study high-energy photon emission from gamma-ray bursts (GRBs). Although the majority of such events (27) have been identified by the Fermi-LAT Collaboration, four were uncovered by using more sensitive statistical techniques. In this paper, we continue our earlier work by finding three more GRBs associated with high-energy photon emission, GRB 110709A, 111117A, and 120107A. To systematize our matched filter approach, a pipeline has been developed to identify these objects in nearly real time. GRB 120107A is the first product of this analysis procedure. Despite the reduced threshold for identification, the number of GRB events has not increased significantly. This relative dearth of events with low photon number prompted a study of the apparent photon number distribution. We find an extremely good fit to a simple power law with an exponent of -1.8 +/- 0.3 for the differential distribution. As might be expected, there is a substantial correlation between the number of lower energy photons detected by the Gamma-ray Burst Monitor (GBM) and the number observed by LAT. Thus, high-energy photon emission is associated with some but not all of the brighter GBM events. Deeper studies of the properties of the small population of high-energy emitting bursts may eventually yield a better understanding of these entire phenomena.
C1 [Zheng, WeiKang; Akerlof, Carl W.; McKay, Timothy A.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Pandey, Shashi B.] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, India.
[Zhang, BinBin] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Zhang, Bing] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Sakamoto, Takanori] NASA, Ctr Res & Explorat Space Sci & Technol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sakamoto, Takanori] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
RP Zheng, WK (reprint author), Univ Michigan, Dept Phys, 450 Church St, Ann Arbor, MI 48109 USA.
EM zwk@umich.edu
RI McKay, Timothy/C-1501-2009; Zhang, Binbin/C-9035-2013
OI McKay, Timothy/0000-0001-9036-6150; Zhang, Binbin/0000-0003-2002-116X
FU NASA [NNX08AV63G]; NSF [PHY-0801007]
FX We thank the anonymous referee for helpful comments and suggestions for
improving this manuscript. We gratefully acknowledge the assistance of
Valerie Connaughton at the Marshall Space Flight Center and Chris
Shrader at the Fermi Science Support Center for their help in obtaining
specific GBM data and providing information about some detailed aspects
of the Fermi mission. This research is supported by the NASA Grant
NNX08AV63G and the NSF Grant PHY-0801007.
NR 32
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2012
VL 756
IS 1
AR 64
DI 10.1088/0004-637X/756/1/64
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009SA
UT WOS:000309044300064
ER
PT J
AU Huth, T
Porder, S
Chaves, J
Whiteside, JH
AF Huth, Timothy
Porder, Stephen
Chaves, Joaquin
Whiteside, Jessica H.
TI Soil Carbon and Nutrient Changes Associated with Deforestation for
Pasture in Southern Costa Rica
SO BIOTROPICA
LA English
DT Article
DE cattle; deforestation; nutrients; pasture; soil carbon; terracettes
ID LAND-USE CHANGE; FOREST; STOCKS; AGRICULTURE; CONSTRAINTS; ATMOSPHERE;
FERTILITY; RETENTION; AMAZONIA; DYNAMICS
AB We assessed the effects of deforestation on soil carbon (C) and nutrient stocks in the premontane landscape near Las Cruces Biological Station in southern Costa Rica, where forests were cleared for pasture in the mid-1960s. We excavated six soil pits to a depth of 1 similar to m in both pasture and primary forest, and found that C stocks were similar to 20 similar to kg similar to C/m2 in both settings. Nevertheless, soil d13C suggests similar to 50 percent of the forest-derived soil C above 40 similar to cm depth has turned over since deforestation. Soil nitrogen (N) and phosphorus (P) stocks derived from the soil pits were not significantly different between land uses (P similar to=similar to 0.43 and 0.61, respectively). At a larger spatial scale, however, the ubiquity of ruts produced by cattle-induced erosion indicates that there are substantial soil effects of grazing in this steep landscape. Ruts averaged 13 similar to cm deep and covered similar to 45 percent of the landscape, and thus are evidence of the removal of 0.7 similar to Mg similar to C/ha/yr, and 70, 9 and 40 similar to kg/ha/yr of N, P and potassium (K), respectively. Subsoils in this region are similar to 10 times less C- and N-rich, and similar to 2 times less P- and K-rich than the topsoil. Thus, rapid topsoil loss may lead to a decline in pasture productivity in the coming decades. These data also suggest that the soil C footprint of deforestation in this landscape may be determined by the fate of soil C as it is transported downstream, rather than C turnover in situ.
C1 [Porder, Stephen] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA.
[Huth, Timothy] Brown Univ, Ctr Environm Studies, Providence, RI 02912 USA.
[Chaves, Joaquin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Whiteside, Jessica H.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
RP Porder, S (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA.
EM stephen_porder@brown.edu
FU Andrew Mellon Foundation; NSF DEB [0918387]
FX We would like to thank Zak Zahawi and the staff of the Las Cruces
Biological Station for their support in the field. This research was
supported by the Andrew Mellon Foundation and NSF DEB 0918387 to S.P.
NR 32
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U1 4
U2 45
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0006-3606
J9 BIOTROPICA
JI Biotropica
PD SEP
PY 2012
VL 44
IS 5
BP 661
EP 667
DI 10.1111/j.1744-7429.2012.00863.x
PG 7
WC Ecology
SC Environmental Sciences & Ecology
GA 000QW
UT WOS:000308403400011
ER
PT J
AU Liu, Z
Ostrenga, D
Teng, W
Kempler, S
AF Liu, Zhong
Ostrenga, Dana
Teng, William
Kempler, Steven
TI Tropical Rainfall Measuring Mission (TRMM) Precipitation Data and
Services for Research and Applications
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID RADAR; VISUALIZATION; SYSTEMS
C1 [Liu, Zhong] George Mason Univ, CSISS, Fairfax, VA 22030 USA.
[Ostrenga, Dana] ADNET Syst, Rockville, MD USA.
[Teng, William] Wyle Informat Syst, Mclean, VA USA.
[Kempler, Steven] NASA, Goddard Earth Sci GES Data & Informat Serv Ctr DI, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Liu, Z (reprint author), George Mason Univ, CSISS, 4400 Univ Dr, Fairfax, VA 22030 USA.
EM Zhong.Liu@nasa.gov
RI Measurement, Global/C-4698-2015
NR 29
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U1 0
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD SEP
PY 2012
VL 93
IS 9
BP 1317
EP 1325
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 009WP
UT WOS:000309056400002
ER
PT J
AU Strong, K
Saba, J
Kucera, T
AF Strong, Keith
Saba, Julia
Kucera, Therese
TI UNDERSTANDING SPACE WEATHER: THE SUN AS A VARIABLE STAR
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID TIME-DISTANCE HELIOSEISMOLOGY; SOLAR OSCILLATIONS
C1 [Strong, Keith; Saba, Julia] SP Syst Inc, Greenbelt, MD USA.
[Strong, Keith; Saba, Julia] Univ Maryland, College Pk, MD 20742 USA.
[Kucera, Therese] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Strong, K (reprint author), 12310 Longwater Dr, Bowie, MD 20721 USA.
EM drkts@aol.com
FU NASA Goddard Space Flight Center via SP Systems, Inc. [670]; University
of Maryland, College Park
FX We have benefited from constructive discussions with Jack Harvey (NSO),
Joan Schmelz (University of Memphis), and Karen Fox (ADNET Systems,
Inc., at NASA GSFC). This work was made possible by support from Code
670 at NASA Goddard Space Flight Center via SP Systems, Inc., and the
University of Maryland, College Park.
NR 23
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U1 0
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD SEP
PY 2012
VL 93
IS 9
BP 1327
EP 1335
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 009WP
UT WOS:000309056400003
ER
PT J
AU Strange, M
AF Strange, Maxwell
TI Buffers stabilize oscillator
SO EDN
LA English
DT Editorial Material
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Strange, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU CANON COMMUNICATIONS INC
PI LOS ANGELES
PA 11444 W OLYMPIC BLVD, SUITE 900, LOS ANGELES, CA 90064 USA
SN 0012-7515
J9 EDN
JI EDN
PD SEP
PY 2012
VL 57
IS 15
BP 59
EP 59
PG 1
WC Engineering, Electrical & Electronic
SC Engineering
GA 012QN
UT WOS:000309251700013
ER
PT J
AU Chu, E
Goebel, DM
AF Chu, Emily
Goebel, Dan M.
TI High-Current Lanthanum Hexaboride Hollow Cathode for 10-to-50-kW Hall
Thrusters
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Cathodes; electron emission; plasma devices; space technology
ID WORK FUNCTION; FILAMENTS
AB Space missions continue to demand higher power Hall thrusters that provide high thrust and long life. For in-space propulsion applications such as high-power orbit raising and cargo missions, Hall thrusters capable of operating in the range of 10-50 kW are in development. The hollow cathodes for these thrusters will be required to produce discharge currents of 20-100 A with lifetimes well in excess of 10 kh. A lanthanum hexaboride (LaB6) hollow cathode with these capabilities has been developed that features graphite tubes or sleeves to provide a diffusion boundary that protects the LaB6 electron emitter from chemical reactions with the refractory metal support structure and includes a long-life heater capable of igniting the high-temperature electron emitter. Cathode operation has been fully characterized at currents of 20-100 A including probe measurements of the plasma parameters inside the LaB6 insert and energetic ion measurements in the cathode plume. The cathode was also tested at up to 200 A of discharge current to explore the cathode failure mechanisms. While the LaB6 cathode operates at higher temperatures than conventional barium oxide-impregnated dispenser cathode, LaB6 provides very high discharge currents, long life, and significantly less sensitivity to propellant impurities and air exposure than conventional dispenser cathodes.
C1 [Chu, Emily] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Chu, Emily; Goebel, Dan M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chu, E (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
EM emily.chu@jpl.nasa.gov; dan.m.goebel@jpl.nasa.gov
NR 46
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U1 0
U2 31
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD SEP
PY 2012
VL 40
IS 9
BP 2133
EP 2144
DI 10.1109/TPS.2012.2206832
PG 12
WC Physics, Fluids & Plasmas
SC Physics
GA 004DF
UT WOS:000308659600005
ER
PT J
AU Cross, M
Varhue, W
Valdez, T
AF Cross, Michael
Varhue, Walter
Valdez, Thomas
TI Structure and electro-catalytic properties of electrode materials
consisting of Pt nanorod decorated/RuO2 nanorod coated substrates
SO INTERNATIONAL JOURNAL OF HYDROGEN ENERGY
LA English
DT Article
DE Electrolysis; Hydrogen production; Nanorods; RuO2; Pt nanoclusters
ID HYDROGEN EVOLUTION REACTION; ELECTROCATALYTIC PERFORMANCE;
NANOPARTICLES; FUEL; NANOWIRES; ENERGY; WATER; CYCLE
AB Nanorod coated materials have the potential of being exceptional electro-catalysts. In this investigation Pt nanorod decorated ruthenium dioxide square nanorods have been grown on aluminized Si substrates and used as the cathode in a system to electrolyze a [2M] aqueous solution of KOH. Gaseous hydrogen was produced at the cathode. The voltage measured at the cathode relative to the solution, and that across both electrodes was found to be dependent on the cathode material used. At a current density of 30 mA/cm(2), the potential drop from the cathode electrode to the liquid electrolyte was measured to be -0.72 V for a solid Pt electrode and -0.69 V for the best Pt nanorod coated electrode. Copyright (C) 2012, Hydrogen Energy Publications, LLC. Published by Elsevier Ltd. All rights reserved.
C1 [Cross, Michael; Varhue, Walter] Univ Vermont, Sch Engn, Burlington, VT 05405 USA.
[Valdez, Thomas] NASA JPL, Electrochem Technol Grp, Pasadena, CA 91109 USA.
RP Cross, M (reprint author), Univ Vermont, Sch Engn, Burlington, VT 05405 USA.
EM mcross1@uvm.edu
FU Navy, Office of Naval Research
FX We would like to thank Mr. Stephen Mongeon of IBM Microelectronics for
assistance in TEM imaging. We are grateful to the Navy, Office of Naval
Research who sponsored the research.
NR 26
TC 0
Z9 0
U1 3
U2 20
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0360-3199
J9 INT J HYDROGEN ENERG
JI Int. J. Hydrog. Energy
PD SEP
PY 2012
VL 37
IS 18
BP 13256
EP 13262
DI 10.1016/j.ijhydene.2012.07.005
PG 7
WC Chemistry, Physical; Electrochemistry; Energy & Fuels
SC Chemistry; Electrochemistry; Energy & Fuels
GA 009RP
UT WOS:000309043200003
ER
PT J
AU Steenburgh, WJ
Massey, JD
Painter, TH
AF Steenburgh, W. James
Massey, Jeffrey D.
Painter, Thomas H.
TI Episodic Dust Events of Utah's Wasatch Front and Adjoining Region
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID WESTERN UNITED-STATES; SPATIAL CHARACTERISTICS; COLORADO PLATEAU;
NORTH-AMERICA; AIR-POLLUTION; MOJAVE DESERT; STORMS; CLIMATE;
VELOCITIES; TRANSPORT
AB Episodic dust events cause hazardous air quality along Utah's Wasatch Front and dust loading of the snowpack in the adjacent Wasatch Mountains. This paper presents a climatology of episodic dust events of the Wasatch Front and adjoining region that is based on surface weather observations from the Salt Lake City International Airport (KSLC), Geostationary Operational Environmental Satellite (GOES) imagery, and additional meteorological datasets. Dust events at KSLC-defined as any day [mountain standard time (MST)] with at least one report of a dust storm, blowing dust, and/or dust in suspension with a visibility of 10 km or less-average 4.3 per water year (WY: October-September), with considerable interannual variability and a general decline in frequency during the 1930-2010 observational record. The distributions of monthly dust-event frequency and total dust flux are bimodal, with primary and secondary maxima in April and September, respectively. Dust reports are most common in the late afternoon and evening. An analysis of the 33 most recent (2001-10 WY) events at KSLC indicates that 11 were associated with airmass convection, 16 were associated with a cold front or baroclinic trough entering Utah from the west or northwest, 4 were associated with a stationary or slowly moving front or baroclinic trough west of Utah, and 2 were associated with other synoptic patterns. GOES imagery from these 33 events, as well as 61 additional events from the surrounding region, illustrates that emission sources are located primarily in low-elevation Late Pleistocene-Holocene alluvial environments in southern and western Utah and southern and western Nevada.
C1 [Steenburgh, W. James; Massey, Jeffrey D.] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT 84112 USA.
[Painter, Thomas H.] Jet Prop Lab, Pasadena, CA USA.
RP Steenburgh, WJ (reprint author), Univ Utah, Dept Atmospher Sci, 135 S 1460 E,Rm 819, Salt Lake City, UT 84112 USA.
EM jim.steenburgh@utah.edu
RI Painter, Thomas/B-7806-2016
FU National Science Foundation [AGS-0627937]; NASA [NNX10AO97G]; USDA
Forest Service Agreement [10-PA-11041914-045]
FX We thank Trevor Alcott for his contributions to the KSLC dust-event
climatology and Paul Jewell for assisting with the identification of
dust emission sources. John Lewis and two anonymous referees provided
reviews that helped to improve the manuscript. We gratefully acknowledge
the provision of datasets, software, and/or computer time and services
by NCEP, NCAR, Unidata, the Center for Ocean-Land-Atmosphere Studies,
and the University of Utah Center for High Performance Computing. This
research was supported by National Science Foundation Grant AGS-0627937,
NASA Grant NNX10AO97G, and USDA Forest Service Agreement
10-PA-11041914-045. Any opinions, findings, and conclusions or
recommendations expressed in this paper are those of the authors and do
not necessarily reflect the views of the National Science Foundation,
NASA, or the USDA Forest Service.
NR 66
TC 21
Z9 21
U1 2
U2 22
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD SEP
PY 2012
VL 51
IS 9
BP 1654
EP 1669
DI 10.1175/JAMC-D-12-07.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 003TG
UT WOS:000308633600006
ER
PT J
AU Misra, A
Tripathi, SN
Kaul, DS
Welton, EJ
AF Misra, Amit
Tripathi, S. N.
Kaul, D. S.
Welton, Ellsworth J.
TI Study of MPLNET-Derived Aerosol Climatology over Kanpur, India, and
Validation of CALIPSO Level 2 Version 3 Backscatter and Extinction
Products
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID GROUND-BASED LIDAR; NORTHERN INDIA; MICROPULSE LIDAR; BLACK CARBON;
SPACE; VARIABILITY; CLOUD; ALGORITHMS; PARAMETERS; NETWORK
AB The level 2 aerosol bacicscatter and extinction profiles from the NASA Micropulse Lidar Network (MPLNET) at Kanpur, India, have been studied from May 2009 to September 2010. Monthly averaged extinction profiles from MPLNET shows high extinction values near the surface during October March. Higher extinction values at altitudes of 2-4 km are observed from April to June, a period marked by frequent dust episodes. Version 3 level 2 Cloud Aerosol Lidar with Orthogonal Polarization (CALIOP) aerosol profile products have been compared with corresponding data from MPLNET over Kanpur for the above-mentioned period. Out of the available back-scatter profiles, the16 profiles used in this study have time differences less than 3 h and distances less than 130 km. Among these profiles, four cases show good comparison above 400 m with R-2 greater than 0.7. Comparison with AERONET data shows that the aerosol type is properly identified by the CALIOP algorithm. Cloud contamination is a possible source of error in the remaining cases of poor comparison. Another source of error is the improper backscatter-to-extinction ratio, which further affects the accuracy of extinction coefficient retrieval.
C1 [Misra, Amit; Tripathi, S. N.; Kaul, D. S.] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India.
[Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Tripathi, SN (reprint author), Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India.
EM snt@iitk.ac.in
RI Tripathi, Sachchida/J-4840-2016
FU DST ICRP; MoES
FX We acknowledge the NOAA/Air Resources Laboratory (ARL) for the provision
of the HYSPLIT transport model and READY website
(http://www.arl.noaa.gov/ready.php) used in this publication. We are
thankful to Atmospheric Science Data Center for providing the CALIOP
level 2 data used in this study. We are grateful to Raymond R. Rogers
(LARC) and Lucia Mona (CNR-IMAA) for useful suggestions regarding
CALIPSO and EARLINET, respectively. This work is financially supported
by DST ICRP and by MoES under a joint (MoES-NERC) program of Changing
Water Cycle.
NR 31
TC 25
Z9 25
U1 1
U2 10
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD SEP
PY 2012
VL 29
IS 9
BP 1285
EP 1294
DI 10.1175/JTECH-D-11-00162.1
PG 10
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 006XT
UT WOS:000308853800009
ER
PT J
AU Bilitza, D
Brown, SA
Wang, MY
Souza, JR
Roddy, PA
AF Bilitza, Dieter
Brown, Steven A.
Wang, Mathew Y.
Souza, Jonas R.
Roddy, Patrick A.
TI Measurements and IRI model predictions during the recent solar minimum
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE IRI; Solar minimum; Ionosonde; C/NOFS
ID INTERNATIONAL REFERENCE IONOSPHERE; HEIGHT
AB Cycle 23 was exceptional in that it lasted almost two years longer than its predecessors and in that it ended in an extended minimum period that proved all predictions wrong. Comparisons of the International Reference Ionosphere (IRI) with CHAMP and GRACE in-situ measurements of electron density during the minimum have revealed significant discrepancies at 400-500 km altitude (Luhr and Xiong, 2010). Our study investigates the causes for these discrepancies with the help of ionosonde and Planar Langmuir Probe (PLP) data from the Communications/Navigation Outage Forecasting System (C/NOFS) satellite. Our C/NOFS comparisons confirm the earlier CHAMP and GRACE results. But the ionosonde measurements of the F-peak plasma frequency (foF2) show generally good agreement throughout the whole solar cycle. At mid-latitude stations yearly averages of the data-model difference are within 10% and at low latitudes stations within 20%. The 60-70% differences found at 400-500 km altitude are not seen at the F peak. We will discuss how these seemingly contradicting results from the ionosonde and insitu data-model comparisons can be explained and which parameters need to be corrected in the IRI model. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Bilitza, Dieter; Brown, Steven A.; Wang, Mathew Y.] George Mason Univ, Space Weather Lab, Fairfax, VA 22030 USA.
[Bilitza, Dieter] NASA GSFC, Heliospher Lab, Greenbelt, MD 20771 USA.
[Souza, Jonas R.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, SP, Brazil.
[Roddy, Patrick A.] USAF, Space Vehicles Directorate, Res Lab, Hanscom Afb, MA USA.
RP Bilitza, D (reprint author), George Mason Univ, Space Weather Lab, Fairfax, VA 22030 USA.
EM dbilitza@gmu.edu; jonas@dae.inpe.br; Patrick.Roddy@hanscom.af.mil
RI Souza, Jonas/B-3514-2013
FU NASA [NNX09AJ74G]; NSF [ATM-0819440]
FX DB and SB acknowledge support through NASA grant NNX09AJ74G and NSF
grant ATM-0819440. The ionosonde data were obtained from NOAA's National
Geophysical Data Center except for the Brazilian data, which were
provided by JRS.
NR 19
TC 38
Z9 39
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD SEP
PY 2012
VL 86
BP 99
EP 106
DI 10.1016/j.jastp.2012.06.010
PG 8
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 013GS
UT WOS:000309294500012
ER
PT J
AU Zhim, F
Ayers, RA
Moore, JJ
Moufarrege, R
Yahia, L
AF Zhim, Fouad
Ayers, Reed A.
Moore, John J.
Moufarrege, Richard
Yahia, L'Hocine
TI Personalized implant for high tibial opening wedge: Combination of solid
freeform fabrication with cdombustion synthesis process
SO JOURNAL OF BIOMATERIALS APPLICATIONS
LA English
DT Article
DE Osteotomy wedge; bioceramic; rapid prototyping; combustion synthesis
ID TRICALCIUM PHOSPHATE; COMBUSTION SYNTHESIS; OSTEOTOMY
AB In this work a new generation of bioceramic personalized implants were developed. This technique combines the processes of solid freeform fabrication (SFF) and combustion synthesis (CS) to create personalized bioceramic implants with tricalcium phosphate (TCP) and hydroxyapatite (HA). These porous bioceramics will be used to fill the tibial bone gap created by the opening wedge high tibial osteotomy (OWHTO). A freeform fabrication with three-dimensional printing (3DP) technique was used to fabricate a metallic mold with the same shape required to fill the gap in the opening wedge osteotomy. The mold was subsequently used in a CS process to fabricate the personalized ceramic implants with TCP and HA compositions. The mold geometry was designed on commercial 3D CAD software. The final personalized bioceramic implant was produced using a CS process. This technique was chosen because it exploits the exothermic reaction between P2O5 and CaO. Also, chemical composition and distribution of pores in the implant could be controlled. To determine the chemical composition, the microstructure, and the mechanical properties of the implant, cylindrical shapes were also fabricated using different fabrication parameters. Chemical composition was performed by X-ray diffraction. Pore size and pore interconnectivity was measured and analyzed using an electronic microscope system. Mechanical properties were determined by a mechanical testing system. The porous TCP and HA obtained have an open porous structure with an average 400 mu m channel size. The mechanical behavior shows great stiffness and higher load to failure for both ceramics. Finally, this personalized ceramic implant facilitated the regeneration of new bone in the gap created by OWHTO and provides additional strength to allow accelerated rehabilitation.
C1 [Zhim, Fouad; Yahia, L'Hocine] Ecole Polytech Montreal, Lab Innovat & Anal Bioperformance LIAB, Montreal, PQ H3T 1J4, Canada.
[Ayers, Reed A.; Moore, John J.] Colorado Sch Mines, NASA, Adv Combust Synth & Engn Lab ACSEL, Golden, CO 80401 USA.
[Moufarrege, Richard] Univ Montreal, Dept Med, Montreal, PQ A1L 1C1, Canada.
RP Zhim, F (reprint author), Ecole Polytech Montreal, Lab Innovat & Anal Bioperformance LIAB, Montreal, PQ H3T 1J4, Canada.
EM fouad.zhim@polymtl.ca
FU CRSNG/NSERC
FX The authors would like to thank the CRSNG/NSERC for its support and Pr.
Carl-Eric Aubin from Centre de recherche du CHU Sainte-Justine,
Montreal.
NR 19
TC 3
Z9 3
U1 1
U2 25
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0885-3282
EI 1530-8022
J9 J BIOMATER APPL
JI J. Biomater. Appl.
PD SEP
PY 2012
VL 27
IS 3
BP 323
EP 332
DI 10.1177/0885328211404938
PG 10
WC Engineering, Biomedical; Materials Science, Biomaterials
SC Engineering; Materials Science
GA 993EP
UT WOS:000307838900008
PM 21750185
ER
PT J
AU Robertson, FR
Roberts, JB
AF Robertson, Franklin R.
Roberts, Jason B.
TI Intraseasonal Variability in MERRA Energy Fluxes over the Tropical
Oceans
SO JOURNAL OF CLIMATE
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; SEA-SURFACE TEMPERATURE; CLOUD-RESOLVING
MODEL; PACIFIC WARM POOL; VERTICAL STRUCTURE; ARAKAWA-SCHUBERT; WESTERN
PACIFIC; CLIMATE MODELS; INDIAN OCEANS; GLOBAL-SCALE
AB This paper investigates intraseasonal variability as represented by the recent NASA Global Modeling and Assimilation Office (GMAO) reanalysis, the Modern-Era Retrospective analysis for Research and Applications (MERRA). The authors examine the behavior of heat, moisture, and radiative fluxes emphasizing their contribution to intraseasonal variations in heat and moisture balance integrated over the tropical oceans. MERRA successfully captures intraseasonal signals in both state variables and fluxes, though it depends heavily on the analysis increment update terms that constrain the reanalysis to be near the observations. Precipitation anomaly patterns evolve in close agreement with those from the Tropical Rainfall Measuring Mission (TRMM) though locally MERRA may occasionally be smaller by up to 20%. As in the TRMM observations, tropical convection increases lead tropospheric warming by approximately 7 days. Radiative flux anomalies are dominated by cloud forcing and are found to replicate the top-of-the-atmosphere (TOA) energy loss associated with increased convection found by other observationally based studies. However, MERRA's convectively produced clouds appear to deepen too soon as precipitation increases. Total fractional cloud cover variations appear somewhat weak compared to observations from the Moderate Resolution Imaging Spectroradiometer (MODIS). Evolution of the surface fluxes, convection, and TOA radiation is consistent with the "discharge-recharge'' paradigm that posits the importance of lower-tropospheric moisture accumulation prior to the expansion of organized deep convection. The authors conclude that MERRA constitutes a very useful representation of intraseasonal variability that will support a variety of studies concerning radiative-convective-dynamical processes and will help identify pathways for improved moist physical parameterization in global models.
C1 [Robertson, Franklin R.; Roberts, Jason B.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA.
RP Robertson, FR (reprint author), NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA.
EM pete.robertson@nasa.gov
FU NASA Earth Science MEaSUREs DISCOVER Project
FX This study was supported by the NASA Modeling Analysis and Prediction
(MAP), Dr. David Considine, Program Manager, and by the NASA Energy and
Water Cycle Study (NEWS) Program, Dr. Jared Entin, Program Manager. The
authors thank Dr. Michael Bosilovich for discussions regarding MERRA and
the anonymous reviewers for comments that improved an earlier version of
the manuscript. Daily MERRA fields were acquired from the Goddard Earth
Sciences (GES) Data and Information Services Center
(http://disc.sci.gsfc.nasa.gov). AMSU-A channel-5 brightness temperature
data were obtained from the Global Hydrology Resource Center
(http://ghrc.nsstc.nasa.gov). Near-surface meteorology and ocean
turbulent fluxes were obtained from the objectively analyzed air-sea
fluxes for the global ocean (OAFLux) dataset
(http://oaflux//modis-atmos.gsfc.nasa.gov/MOD08_D3.whoi.edu/). TOA and
surface radiative fluxes were provided by the NASA/GEWEX Surface
Radiation Project and obtained from the NASA Langley Research Center
Atmospheric Sciences Data Center. TRMM PR 3G68 and 3B42 datasets were
acquired from the Goddard Distributed Active Archive Center
(ftp://trmmopen.gsfc.nasa.gov/pub/). TMI column water vapor is produced
by Remote Sensing Systems and sponsored by the NASA Earth Science
MEaSUREs DISCOVER Project (data are available online at www.remss.com).
MODIS cloud optical thickness came from collection 005 MOD08_D3 dataset
(http://modis-atmos.gsfc.nasa.gov/MOD08_D3).
NR 63
TC 6
Z9 6
U1 0
U2 7
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 SEP 1
PY 2012
VL 25
IS 17
BP 5629
EP 5647
DI 10.1175/JCLI-D-11-00428.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 003TF
UT WOS:000308633500001
ER
PT J
AU Del Genio, AD
Wu, JB
Chen, YH
AF Del Genio, Anthony D.
Wu, Jingbo
Chen, Yonghua
TI Characteristics of Mesoscale Organization in WRF Simulations of
Convection during TWP-ICE
SO JOURNAL OF CLIMATE
LA English
DT Article
ID INTERNATIONAL CLOUD EXPERIMENT; HIGH-RESOLUTION SIMULATION; TRMM
PRECIPITATION RADAR; INCLUDING MASS FLUXES; DEEP CONVECTION; CLIMATE
MODELS; SQUALL-LINE; WARM POOL; PART II; STRATIFORM PRECIPITATION
AB Compared to satellite-derived heating profiles, the Goddard Institute for Space Studies general circulation model (GCM) convective heating is too deep and its stratiform upper-level heating is too weak. This deficiency highlights the need for GCMs to parameterize the mesoscale organization of convection. Cloud-resolving model simulations of convection near Darwin, Australia, in weak wind shear environments of different humidities are used to characterize mesoscale organization processes and to provide parameterization guidance. Downdraft cold pools appear to stimulate further deep convection both through their effect on eddy size and vertical velocity. Anomalously humid air surrounds updrafts, reducing the efficacy of entrainment. Recovery of cold pool properties to ambient conditions over 5-6 h proceeds differently over land and ocean. Over ocean increased surface fluxes restore the cold pool to prestorm conditions. Over land surface fluxes are suppressed in the cold pool region; temperature decreases and humidity increases, and both then remain nearly constant, while the undisturbed environment cools diurnally. The upper-troposphere stratiform rain region area lags convection by 5- 6 h under humid active monsoon conditions but by only 1-2 h during drier break periods, suggesting that mesoscale organization is more readily sustained in a humid environment. Stratiform region hydrometeor mixing ratio lags convection by 0-2 h, suggesting that it is strongly influenced by detrainment from convective updrafts. Small stratiform region temperature anomalies suggest that a mesoscale updraft parameterization initialized with properties of buoyant detrained air and evolving to a balance between diabatic heating and adiabatic cooling might be a plausible approach for GCMs.
C1 [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wu, Jingbo; Chen, Yonghua] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM anthony.d.delgenio@nasa.gov
OI Del Genio, Anthony/0000-0001-7450-1359
FU NASA Precipitation Measurement Missions program; DOE Atmospheric System
Research program; FASTER program; NASA Modeling, Analysis, and
Prediction program
FX This research was supported by the NASA Precipitation Measurement
Missions program, the DOE Atmospheric System Research and FASTER
programs, and the NASA Modeling, Analysis, and Prediction program. We
thank two anonymous reviewers for their constructive suggestions, which
improved the paper.
NR 77
TC 29
Z9 29
U1 0
U2 11
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 SEP 1
PY 2012
VL 25
IS 17
BP 5666
EP 5688
DI 10.1175/JCLI-D-11-00422.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 003TF
UT WOS:000308633500003
ER
PT J
AU Wang, TS
Lin, J
Ruf, J
Guidos, M
Cheng, GC
AF Wang, Ten-See
Lin, Jeff
Ruf, Joe
Guidos, Mike
Cheng, Gary C.
TI Effect of Coolant Flow Distribution on Transient Side Load of
Film-Cooled Nozzles
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID ENGINE NOZZLE; SEPARATION; PERFORMANCE; SIMULATION; REGIME
AB The objective of this study was to investigate the effect of film-coolant distribution on nozzle side loads generated during an engine start transient. The rocket engine studied encompasses a regeneratively cooled chamber and nozzle, along with a film-cooled nozzle extension. The computational methodology is based on an unstructured-grid pressure-based computational fluid dynamics formulation and transient inlet boundary conditions calculated from an engine system simulation. Computations were performed for engine startup with two turbine exhaust manifold geometries that produce two different distributions of film-coolant mass flow: one with a higher mass flow deviation, and the other with a near uniform distribution. The results show that the configuration with the higher mass flow deviation produced a higher peak side load, manifested by the biased turbine exhaust gas pumping of the supersonic jet of the Mach disk flow; the configuration with the more uniform coolant flow distribution maintained a more symmetric Mach disk flow throughout the filling process, resulting in a lower peak side load.
C1 [Wang, Ten-See; Lin, Jeff; Ruf, Joe] NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch, Prop Struct Thermal & Fluids Anal Div, Huntsville, AL 35812 USA.
[Cheng, Gary C.] Univ Alabama Birmingham, Dept Mech Engn, Birmingham, AL 35294 USA.
[Guidos, Mike] NASA, George C Marshall Space Flight Ctr, Liquid Engine & Main Prop Syst Branch, Prop Syst Design & Integrat Div, Huntsville, AL 35812 USA.
RP Wang, TS (reprint author), NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch, Prop Struct Thermal & Fluids Anal Div, ER42, Huntsville, AL 35812 USA.
FU J-2X Engine Program at NASA Marshall Space Flight Center
FX The efforts from the first four authors were supported by the J-2X
Engine Program at NASA Marshall Space Flight Center. The fifth author,
along with Yen-Sen Chen of National Applied Research Laboratories and
Yasushi Ito of University of Alabama at Birmingham, provided timely
codes and software support. The lead author wishes to thank Mike Shadoan
for his support of the task and James Beck of Pratt and Whitney
Aircraft, United Technologies Corporation, for his interest in this
task. The fourth coauthor wishes to thank Duc Nguyen and Danny Woo of
Pratt and Whitney Aircraft, United Technologies Corporation, for
providing the engine design and transient sequencing information
necessary to create the NASA Marshall Space Flight Center J-2X engine
system model.
NR 32
TC 3
Z9 3
U1 0
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
J9 J PROPUL POWER
JI J. Propul. Power
PD SEP-OCT
PY 2012
VL 28
IS 5
BP 1081
EP 1090
DI 10.2514/1.B34397
PG 10
WC Engineering, Aerospace
SC Engineering
GA 007NU
UT WOS:000308896200021
ER
PT J
AU Bruna, D
Cravero, C
Turner, MG
Merchant, A
AF Bruna, Dario
Cravero, Carlo
Turner, Mark G.
Merchant, Ali
TI An Educational Software Suite for Teaching Design Strategies for
Multistage Axial Flow Compressors
SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME
LA English
DT Article
AB The T-AXI turbomachinery design system, an axisymmetric methodology recently developed with an educational purpose, has shown great capabilities in the redesign of existing axial flow gas turbine components. Different turbomachines, single or multistage configurations, have been already reproduced with excellent overall performance results: examples are the NASA/GE E 3 HP compressor and LP turbine. In this paper, the authors present a detailed analysis of the results of a "case-study" application of the code as a complementary tool to be used during a turbomachinery design course. The NASA/GE E 3 HP compressor has been chosen as the test case. Starting from the data available in open literature the different steps of the redesign have been reported: from the flowpath generation through the thermodynamic properties distributions to the overall turbomachine performance analysis. Particular attention has been given to some critical aero design parameters. The links to some interesting and useful literature sources are reported. The free-vortex, the only vortex law included in the first version of the code has been used for a first EEE compressor redesign. Different design vortex methodologies have been implemented in the new release of the code and their effects on the angular momentum are reported. The corresponding geometries can also be interfaced to a mesh generator and then the turbomachinery configurations analyzed by a 3D Navier-Stokes solver. In this way the flow field can be carefully analyzed and the fluid-dynamic physics better understood. With the above software structure the student has the opportunity to test the effects of different design strategies on the turbomachinery performance and to understand the need of a hierarchy of tools that give complete information for the multistage turbomachinery design. Finally, in the last section of the paper, the authors present how a project such as T-AXI, developed from their research activity in turbomachinery, numerical methods and CFD, can be included in the education tool CompEdu. [DOI: 10.1115/1.4003831]
C1 [Bruna, Dario] NASA, Glenn Res Ctr, Turbomachinery & Heat Transfer Branch, Cleveland, OH 44142 USA.
[Cravero, Carlo] Univ Genoa, DIMSET, I-16145 Genoa, GE, Italy.
[Turner, Mark G.] Univ Cincinnati, Dept Aerosp Engn & Engn Mech, Cincinnati, OH 45221 USA.
[Merchant, Ali] CADNexus, Arlington, MA 02476 USA.
RP Bruna, D (reprint author), NASA, Glenn Res Ctr, Turbomachinery & Heat Transfer Branch, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
EM dariobruna@fastwebnet.it; cravero@unige.it; mark.turner@uc.edu;
merchant@cadnexus.com
NR 13
TC 1
Z9 1
U1 1
U2 6
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0889-504X
J9 J TURBOMACH
JI J. Turbomach.-Trans. ASME
PD SEP
PY 2012
VL 134
IS 5
AR 051010
DI 10.1115/1.4003831
PG 8
WC Engineering, Mechanical
SC Engineering
GA 000RE
UT WOS:000308404500010
ER
PT J
AU Bi, HS
Peterson, WT
Peterson, JO
Fisher, JL
AF Bi, Hongsheng
Peterson, William T.
Peterson, Jay O.
Fisher, Jennifer L.
TI A comparative analysis of coastal and shelf-slope copepod communities in
the northern California Current system: Synchronized response to
large-scale forcing?
SO LIMNOLOGY AND OCEANOGRAPHY
LA English
DT Article
ID CENTRAL OREGON COAST; ZOOPLANKTON COMMUNITY; CLIMATE-CHANGE; OCEAN;
ECOSYSTEM; PACIFIC; BIODIVERSITY; VARIABILITY; PERSISTENCE; EUPHAUSIIDS
AB The synchrony between coastal and shelf-slope copepod communities was investigated in the northern California Current (NCC) system, a strong upwelling zone, using time series of zooplankton sampled from a nearshore station (9 km offshore, water depth 62 m) and a shelf-slope station (46 km offshore, water depth 297 m). Long-term trends and seasonal changes were constructed for the dissimilarity index (Euclidean distance) between the two stations and for the biomass of three different copepod assemblages at the two stations: cold neritic, southern, and warm neritic copepods. The dissimilarity between the community structures of the two stations showed little variation in the long-term trend, but exhibited a clear seasonal pattern. All three copepod assemblages showed similar long-term trends in relation to the large-scale forcing as indexed by the Pacific Decadal Oscillation at both stations, but variations in the long-term trend at the nearshore station were much higher than the offshore station. Most copepod groups exhibited regular seasonal patterns at both stations except southern copepods at the nearshore station. All three copepod assemblages exhibited more pronounced seasonal fluctuations at the nearshore station compared with the slope station, and this difference is likely driven by higher productivity nearshore fueled by nutrient-enriched upwelled water. Copepods in the inshore and offshore waters in the NCC ecosystem showed synchronized response to the large-scale variability in physical forcing and copepods in the coastal waters were more responsive to local perturbations than were those in the slope waters.
C1 [Bi, Hongsheng] Univ Maryland, Chesapeake Biol Lab, Ctr Environm Sci, Solomons, MD 20688 USA.
[Peterson, William T.] Natl Marine Fisheries Serv, Newport Stn, Hatfield Marine Sci Ctr, Newport, OR USA.
[Peterson, Jay O.; Fisher, Jennifer L.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
RP Bi, HS (reprint author), Univ Maryland, Chesapeake Biol Lab, Ctr Environm Sci, Solomons, MD 20688 USA.
EM hbi@umces.edu
RI Bi, Hongsheng/B-9409-2012
FU Comparative Analysis of Marine Ecosystem Organization (CAMEO) program
[NA09NMF4720182]; National Oceanographic Partnership Program; Office of
Naval Research; U.S. Global Ocean Ecosystems Dynamics program; National
Marine Fisheries Service Protected Species Stock Assessment Improvement
Plan; Bonneville Power Administration; National Aeronautics and Space
Administration [NNX08AR40G]
FX We thank many people who contributed greatly to the collection and
processing of data: Leah Feinberg, Tracy Shaw, Jennifer Menkel, Hui Liu,
Cheryl Morgan, Rian Hooff, and Karen Hunter. We would also like to thank
the anonymous reviewers for their excellent suggestions. This synthesis
work is supported by the Comparative Analysis of Marine Ecosystem
Organization (CAMEO) program (NA09NMF4720182).; Data collection was
funded by various sources including the National Oceanographic
Partnership Program, the Office of Naval Research, U.S. Global Ocean
Ecosystems Dynamics program, National Marine Fisheries Service Protected
Species Stock Assessment Improvement Plan, and the Bonneville Power
Administration. Some of the data processing was funded by the National
Aeronautics and Space Administration grant NNX08AR40G.
NR 40
TC 2
Z9 2
U1 4
U2 33
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-3590
EI 1939-5590
J9 LIMNOL OCEANOGR
JI Limnol. Oceanogr.
PD SEP
PY 2012
VL 57
IS 5
BP 1467
EP 1478
DI 10.4319/lo.2012.57.5.1467
PG 12
WC Limnology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 003VX
UT WOS:000308640600017
ER
PT J
AU Bennett, M
Bruce, W
AF Bennett, Michael
Bruce, Walt
TI Blow-up space shield beats heat
SO MATERIALS WORLD
LA English
DT Editorial Material
C1 [Bruce, Walt] NASA, Langley Res Ctr, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU I O M COMMUNICATIONS LTD INST MATERIALS
PI LONDON
PA 1 CARLTON HOUSE TERRACE, LONDON SW1Y 5DB, ENGLAND
SN 0967-8638
J9 MATER WORLD
JI Mater. World
PD SEP
PY 2012
VL 20
IS 9
BP 14
EP 14
PG 1
WC Materials Science, Ceramics; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 000LI
UT WOS:000308387400008
ER
PT J
AU Refregier, A
Kacprzak, T
Amara, A
Bridle, S
Rowe, B
AF Refregier, Alexandre
Kacprzak, Tomasz
Amara, Adam
Bridle, Sarah
Rowe, Barnaby
TI Noise bias in weak lensing shape measurements
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; methods: statistical; techniques: image
processing; cosmology: observations; dark energy; dark matter
ID SHEAR ESTIMATION; LIMITATIONS; ALIGNMENTS
AB Weak lensing experiments are a powerful probe into cosmology through their measurement of the mass distribution of the universe. A challenge for this technique is to control systematic errors that occur when measuring the shapes of distant galaxies. In this paper, we investigate noise bias, a systematic error that arises from second-order noise terms in the shape measurement process. We first derive analytical expressions for the bias of general maximum-likelihood estimators in the presence of additive noise. We then find analytical expressions for a simplified toy model in which galaxies are modelled and fitted with a Gaussian with its size as a single free parameter. Even for this very simple case we find a significant effect. We also extend our analysis to a more realistic six-parameter elliptical Gaussian model. We find that the noise bias is generically of the order of the inverse-squared signal-to-noise ratio (SNR) of the galaxies and is thus of the order of a percent for galaxies of SNR 10, i.e. comparable to the weak lensing shear signal. This is nearly two orders of magnitude greater than the systematic requirements for future all-sky weak lensing surveys. We discuss possible ways to circumvent this effect, including a calibration method using simulations discussed in an associated paper.
C1 [Refregier, Alexandre; Amara, Adam] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Kacprzak, Tomasz; Bridle, Sarah; Rowe, Barnaby] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Rowe, Barnaby] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rowe, Barnaby] CALTECH, Pasadena, CA 91106 USA.
RP Refregier, A (reprint author), ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
EM alexandre.refregier@phys.ethz.ch
OI Rowe, Barnaby/0000-0002-7042-9174
FU Royal Society; European Research Council [240672]
FX We thank Gary Bernstein, Julien Carron, Joel Berge, Stephane
Paulin-Henriksson and Lisa Voigt for helpful discussions. SB
acknowledges support from the Royal Society in the form of a University
Research Fellowship, and both SB and BR acknowledge support from the
European Research Council in the form of a Starting Grant with number
240672. Part of BR's work was done at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA.
NR 30
TC 57
Z9 57
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 SEP
PY 2012
VL 425
IS 3
BP 1951
EP 1957
DI 10.1111/j.1365-2966.2012.21483.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 996KC
UT WOS:000308084100021
ER
PT J
AU Pacciani, L
Donnarumma, I
Denney, KD
Assef, RJ
Ikejiri, Y
Yamanaka, M
Uemura, M
Domingo, A
Giommi, P
Tarchi, A
Verrecchia, F
Longo, F
Raino, S
Giusti, M
Vercellone, S
Chen, AW
Striani, E
Vittorini, V
Tavani, M
Bulgarelli, A
Giuliani, A
Pucella, G
Argan, A
Barbiellini, G
Caraveo, P
Cattaneo, PW
Colafrancesco, S
Costa, E
De Paris, G
Del Monte, E
Di Cocco, G
Evangelista, Y
Ferrari, A
Feroci, M
Fiorini, M
Fuschino, F
Galli, M
Gianotti, F
Labanti, C
Lapshov, I
Lazzarotto, F
Lipari, P
Marisaldi, M
Mereghetti, S
Morelli, E
Moretti, E
Morselli, A
Pellizzoni, A
Perotti, F
Piano, G
Picozza, P
Pilia, M
Prest, M
Rapisarda, M
Rappoldi, A
Rubini, A
Sabatini, S
Soffitta, P
Trifoglio, M
Trois, A
Vallazza, E
Zanello, D
Pittori, C
Santolamazza, P
Lucarelli, F
Salotti, L
Valentini, G
AF Pacciani, L.
Donnarumma, I.
Denney, K. D.
Assef, R. J.
Ikejiri, Y.
Yamanaka, M.
Uemura, M.
Domingo, A.
Giommi, P.
Tarchi, A.
Verrecchia, F.
Longo, F.
Raino, S.
Giusti, M.
Vercellone, S.
Chen, A. W.
Striani, E.
Vittorini, V.
Tavani, M.
Bulgarelli, A.
Giuliani, A.
Pucella, G.
Argan, A.
Barbiellini, G.
Caraveo, P.
Cattaneo, P. W.
Colafrancesco, S.
Costa, E.
De Paris, G.
Del Monte, E.
Di Cocco, G.
Evangelista, Y.
Ferrari, A.
Feroci, M.
Fiorini, M.
Fuschino, F.
Galli, M.
Gianotti, F.
Labanti, C.
Lapshov, I.
Lazzarotto, F.
Lipari, P.
Marisaldi, M.
Mereghetti, S.
Morelli, E.
Moretti, E.
Morselli, A.
Pellizzoni, A.
Perotti, F.
Piano, G.
Picozza, P.
Pilia, M.
Prest, M.
Rapisarda, M.
Rappoldi, A.
Rubini, A.
Sabatini, S.
Soffitta, P.
Trifoglio, M.
Trois, A.
Vallazza, E.
Zanello, D.
Pittori, C.
Santolamazza, P.
Lucarelli, F.
Salotti, L.
Valentini, G.
TI The characterization of the distant blazar GB6 J1239+0443 from flaring
and low activity periods
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; galaxies: active; galaxies:
individual: GB6 J1239+0443; quasars: general
ID LARGE-AREA TELESCOPE; BLACK-HOLE MASSES; EXTRAGALACTIC BACKGROUND LIGHT;
GAMMA-RAY SOURCES; GALACTIC NUCLEI; FERMI BLAZARS;
ELECTROMAGNETIC-SPECTRUM; 3C 454.3; EMISSION; MISSION
AB In 2008, AGILE and Fermi detected gamma-ray flaring activity from the unidentified EGRET source 3EG J1236+0457, recently associated with a flat spectrum radio quasar (GB6 J1239+0443) at z = 1.762. The optical counterpart of the gamma-ray source underwent a flux enhancement of a factor of 1530 in six years, and of similar to 10 in six months. We interpret this flare-up in terms of a transition from an accretion-disc-dominated emission to a synchrotron-jet-dominated one. We analysed a Sloan Digital Sky Survey (SDSS) archival optical spectrum taken during a period of low radio and optical activity of the source. We estimated the mass of the central black hole using the width of the C?iv emission line. In our work, we have also investigated SDSS archival optical photometric data and ultraviolet GALEX observations to estimate the thermal disc emission contribution of GB6 J1239+0443. Our analysis of the gamma-ray data taken during the flaring episodes indicates a flat gamma-ray spectrum, with an extension of up to 15?GeV, with no statistically relevant sign of absorption from the broad-line region, suggesting that the blazar zone is located beyond the broad-line region. This result is confirmed by the modelling of the broad-band spectral energy distribution (well constrained by the available multiwavelength data) of the flaring activity periods and by the accretion disc luminosity and black hole mass estimated by us using archival data.
C1 [Denney, K. D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Assef, R. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ikejiri, Y.; Yamanaka, M.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan.
[Uemura, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan.
[Domingo, A.] Ctr Astrobiol INTA CSIC, Madrid 28691, Spain.
[Giommi, P.; Verrecchia, F.; Pittori, C.; Santolamazza, P.; Lucarelli, F.] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Tarchi, A.; Pellizzoni, A.; Pilia, M.; Trois, A.] INAF OAC, I-09012 Capoterra, CA, Italy.
[Longo, F.; Barbiellini, G.; Moretti, E.; Vallazza, E.] Univ Trieste, Dip Fis, I-34127 Trieste, Italy.
[Raino, S.] Ist Nazl Fis Nucl, Sez Bari, I-70125 Bari, Italy.
[Vercellone, S.] INAF IASF Palermo, I-90146 Palermo, Italy.
[Chen, A. W.; Giuliani, A.; Caraveo, P.; Fiorini, M.; Mereghetti, S.; Perotti, F.] INAF IASF Milano, I-20133 Milan, Italy.
[Vittorini, V.; Tavani, M.; Piano, G.; Picozza, P.] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy.
[Bulgarelli, A.; Salotti, L.; Valentini, G.] Agenzia Spaziale Italiana, I-00198 Rome, Italy.
[Pucella, G.; Rapisarda, M.] ENEA Frascati, I-00044 Frascati, Roma, Italy.
[Cattaneo, P. W.; Rappoldi, A.] INFN Pavia, I-27100 Pavia, Italy.
[Colafrancesco, S.] INAF OAR, I-00040 Monte Porzio Catone, Roma, Italy.
[Colafrancesco, S.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg Wits, South Africa.
[Di Cocco, G.; Fuschino, F.; Gianotti, F.; Labanti, C.; Marisaldi, M.; Morelli, E.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Ferrari, A.] Univ Turin, Dip Fis, I-10125 Turin, Italy.
[Galli, M.] ENEA Bologna, I-40129 Bologna, Italy.
[Lipari, P.; Zanello, D.] INFN Roma La Sapienza, I-00185 Rome, Italy.
[Morselli, A.; Piano, G.; Picozza, P.] INFN Roma Tor Vergata, I-00133 Rome, Italy.
[Pilia, M.; Prest, M.] Univ Insubria, Dip Fis, I-22100 Como, Italy.
[Pacciani, L.; Donnarumma, I.; Giusti, M.; Striani, E.; Vittorini, V.; Argan, A.; Costa, E.; De Paris, G.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Lapshov, I.; Lazzarotto, F.; Piano, G.; Rubini, A.; Sabatini, S.; Soffitta, P.] INAF IAPS, I-00133 Rome, Italy.
[Longo, F.; Barbiellini, G.; Moretti, E.; Vallazza, E.] INFN Trieste, I-34127 Trieste, Italy.
RP Pacciani, L (reprint author), INAF IAPS, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM luigi.pacciani@iasf-roma.inaf.it
RI Lazzarotto, Francesco/J-4670-2012; Morselli, Aldo/G-6769-2011; Domingo,
Albert/L-9071-2014; Trifoglio, Massimo/F-5302-2015; Pittori,
Carlotta/C-7710-2016;
OI VALENTINI, Giovanni/0000-0002-2224-1281; Del Monte,
Ettore/0000-0002-3013-6334; trois, alessio/0000-0002-3180-6002;
Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Labanti,
Claudio/0000-0002-5086-3619; Feroci, Marco/0000-0002-7617-3421;
Soffitta, Paolo/0000-0002-7781-4104; Picozza,
Piergiorgio/0000-0002-7986-3321; Vercellone,
Stefano/0000-0003-1163-1396; Fuschino, Fabio/0000-0003-2139-3299;
Caraveo, Patrizia/0000-0003-2478-8018; PREST,
MICHELA/0000-0003-3161-4454; Verrecchia, Francesco/0000-0003-3455-5082;
Gianotti, Fulvio/0000-0003-4666-119X; Lazzarotto,
Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523;
Donnarumma, Immacolata/0000-0002-4700-4549; Sabatini,
Sabina/0000-0003-2076-5767; Marisaldi, Martino/0000-0002-4000-3789;
MEREGHETTI, SANDRO/0000-0003-3259-7801; Tavani,
Marco/0000-0003-2893-1459; Lucarelli, Fabrizio/0000-0002-6311-764X;
Morselli, Aldo/0000-0002-7704-9553; Domingo, Albert/0000-0001-9764-6411;
Trifoglio, Massimo/0000-0002-2505-3630; Pittori,
Carlotta/0000-0001-6661-9779; Tarchi, Andrea/0000-0001-8540-3500;
Pacciani, Luigi/0000-0001-6897-5996; Fiorini, Mauro/0000-0001-8297-1983;
giommi, paolo/0000-0002-2265-5003; Bulgarelli,
Andrea/0000-0001-6347-0649; galli, marcello/0000-0002-9135-3228
FU Italian Space Agency [ASI I/089/06/2]; scientific and programmatic
participation; Italian Institute of Astrophysics (INAF); Italian
Institute of Nuclear Physics (INFN); ASI-INAF [I/009/10/0]
FX We acknowledge financial contribution from the agreement ASI-INAF
I/009/10/0.; The AGILE mission is funded by the Italian Space Agency
(through contract ASI I/089/06/2) with scientific and programmatic
participation by the Italian Institute of Astrophysics (INAF) and the
Italian Institute of Nuclear Physics (INFN).
NR 62
TC 6
Z9 6
U1 1
U2 7
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 SEP
PY 2012
VL 425
IS 3
BP 2015
EP 2026
DI 10.1111/j.1365-2966.2012.21540.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 996KC
UT WOS:000308084100026
ER
PT J
AU Molthan, AL
Colle, BA
AF Molthan, Andrew L.
Colle, Brian A.
TI Comparisons of Single- and Double-Moment Microphysics Schemes in the
Simulation of a Synoptic-Scale Snowfall Event
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID PARTICLE-SIZE DISTRIBUTIONS; BULK PARAMETERIZATION; ICE CLOUDS;
PRECIPITATION PARTICLES; WATER-CONTENT; IN-SITU; MODEL; MESOSCALE;
IMPLEMENTATION; ENSEMBLE
AB The Canadian CloudSat/Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) Validation Project (C3VP) provided aircraft, surface, and remotely sensed observations of cloud and precipitation characteristics to support improved simulation of cold-season precipitation within weather forecast models and new developments in satellite and radar precipitation retrievals. On 22 January 2007, the C3VP campaign executed an intensive observation period to sample widespread snowfall that occurred as a midlatitude cyclone tracked along the U.S.-Canadian border. Surface air temperature and precipitation measurements, combined with aircraft measurement of hydrometeor content and size distribution, are used to examine various assumptions and parameterizations included within four bulk water microphysics schemes available within the Weather Research and Forecasting Model (WRF).
In a simulation of the 22 January 2007 event, WRF forecasts reproduced the overall precipitation pattern observed during aircraft sampling, allowing for a comparison between C3VP measurements and microphysics scheme assumptions. Single-moment schemes that provide flexibility in size distribution parameters as functions of temperature can represent much of the vertical variability observed in aircraft data, but variability is reduced in an environment where the simulated temperature profile is nearly isothermal. Double-moment prediction of total number concentration may improve the representation of ice crystal aggregation. Inclusion of both temperature dependence on distribution parameters and variability in mass-diameter or diameter-fall speed relationships suggest a means of improving upon single-moment predictions.
C1 [Molthan, Andrew L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Colle, Brian A.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
RP Molthan, AL (reprint author), NASA, George C Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM andrew.molthan@nasa.gov
FU Canadian Space Agency; National Science Foundation [ATM-0908288]
FX Model simulations were performed on the NASA Discover Cluster. Data from
the HVSD instrument were provided by GyuWon Lee of McGill University.
Aircraft data were provided through S. Nesbitt (University of Illinois)
with particle size distributions and probe data quality controlled by A.
Heymsfield (NCAR). Prime funding for aircraft studies during the
Canadian CloudSat/CALIPSO Validation Project was provided by the
Canadian Space Agency. Support for data acquisition and related
investigators was provided by the Global Precipitation Measurement
Project (via Dr. M. Schwaller) and the NASA Precipitation Measurement
Mission (via Dr. R. Kakar). This study was supported in part by the
National Science Foundation under Grant ATM-0908288 (Colle). The lead
author would like to thank Greg Thompson of NCAR for several comments
and helpful guidance that improved the analysis and discussion.
Contributions from a second, anonymous reviewer were also helpful for
improving the clarity of discussions regarding aircraft data analysis
and scheme comparisons.
NR 49
TC 17
Z9 17
U1 4
U2 16
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD SEP
PY 2012
VL 140
IS 9
BP 2982
EP 3002
DI 10.1175/MWR-D-11-00292.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 000QA
UT WOS:000308400500014
ER
PT J
AU Liu, TS
Wang, B
Choi, DS
AF Liu, Tianshu
Wang, Bo
Choi, David S.
TI Flow structures of Jupiter's Great Red Spot extracted by using optical
flow method
SO PHYSICS OF FLUIDS
LA English
DT Article
DE astrophysical fluid dynamics; flow visualisation; Jupiter; planetary
atmospheres
ID WHITE OVAL BC; POTENTIAL-VORTICITY; IMAGE VELOCIMETRY; DYNAMICS;
ATMOSPHERE; TRACKING; VELOCITY; GALILEO; FIELDS
AB The flow structures of Jupiter's Great Red Spot (GRS) are studied based on a high-resolution velocity field extracted from the Galileo 1996 cloud images of the GRS by using the physics-based optical flow method. The mean transverse velocity profile across the anti-cyclonic near-elliptical collar of the GRS is obtained. The flow structures in the relatively quiescent inner region enclosed by the high-speed collar are revealed at a coarse-grained level. The cyclonic source node in the inner region is identified that is directly associated with the observed cyclonic rotation near the center of the GRS, and its significance in the maintenance of the GRS is explored by using a topological constraint. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4752227]
C1 [Liu, Tianshu] Western Michigan Univ, Dept Mech & Aeronaut Engn, Kalamazoo, MI 49008 USA.
[Wang, Bo] Univ Elect Sci & Technol China, Sch Math Sci, Chengdu 611731, Peoples R China.
[Choi, David S.] NASA, ORAU, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Liu, TS (reprint author), Western Michigan Univ, Dept Mech & Aeronaut Engn, Kalamazoo, MI 49008 USA.
EM tianshu.liu@wmich.edu
NR 27
TC 4
Z9 4
U1 5
U2 15
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-6631
J9 PHYS FLUIDS
JI Phys. Fluids
PD SEP
PY 2012
VL 24
IS 9
AR 096601
DI 10.1063/1.4752227
PG 13
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 015DN
UT WOS:000309425800039
ER
PT J
AU Matheou, G
Chung, D
AF Matheou, G.
Chung, D.
TI Direct numerical simulation of stratified turbulence
SO PHYSICS OF FLUIDS
LA English
DT Editorial Material
C1 [Matheou, G.; Chung, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Matheou, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Georgios.Matheou@jpl.nasa.gov
RI Chung, Daniel/F-4468-2016
OI Chung, Daniel/0000-0003-3732-364X
NR 1
TC 3
Z9 3
U1 1
U2 8
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-6631
J9 PHYS FLUIDS
JI Phys. Fluids
PD SEP
PY 2012
VL 24
IS 9
AR 091106
DI 10.1063/1.4747156
PG 2
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 015DN
UT WOS:000309425800006
ER
PT J
AU Schwenzer, SP
Abramov, O
Allen, CC
Bridges, JC
Clifford, SM
Filiberto, J
Kring, DA
Lasue, J
McGovern, PJ
Newsom, HE
Treiman, AH
Vaniman, DT
Wiens, RC
Wittmann, A
AF Schwenzer, S. P.
Abramov, O.
Allen, C. C.
Bridges, J. C.
Clifford, S. M.
Filiberto, J.
Kring, D. A.
Lasue, J.
McGovern, P. J.
Newsom, H. E.
Treiman, A. H.
Vaniman, D. T.
Wiens, R. C.
Wittmann, A.
TI Gale Crater: Formation and post-impact hydrous environments
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Gale Crater; Impact-processes; Hydrothermal; Phyllosilicates;
Astrobiology
ID CHICXULUB IMPACT CRATER; HYDROTHERMAL ALTERATION; EARLY MARS; ALTERATION
ASSEMBLAGES; OBLIQUE IMPACTS; EVOLUTION; DIMENSIONS; METEORITES;
HABITATS; SYSTEMS
AB Gale Crater, the landing site of the 2011 Mars Science Laboratory mission, formed in the Late Noachian. It is a 150 km diameter complex impact structure with a central mound (Mount Sharp), the original features of which may be transitional between a central peak and peak ring impact structure. The impact might have melted portions of the substrate to a maximum depth of similar to 17 km and produced a minimum of 3600 km(3) of impact melt, half of which likely remained within the crater. The bulk of this impact melt would have pooled in an annular depression surrounding the central uplift, creating an impact melt pool as thick as 0.5-1 km. The ejecta blanket surrounding Gale may have been as thick as similar to 600 m, which has implications for the amount of erosion that has occurred since Gale Crater formed. After the impact, a hydrothermal system may have been active for several hundred thousand years and a crater lake with associated sediments is likely to have formed. The hydrothermal system, and associated lakes and springs, likely caused mineral alteration and precipitation. In the presence of S-rich host rocks, the alteration phases are modelled to contain sheet silicates, quartz, sulphates, and sulphides. Modelled alteration assemblages may be more complex if groundwater interaction persisted after initial alteration. The warm-water environment might have provided conditions supportive of life. Deep fractures would have allowed for hydraulic connectivity into the deep subsurface, where biotic chemistry (and possibly other evidence of life) may be preserved. (c) 2012 Elsevier Ltd. All rights reserved.
C1 [Schwenzer, S. P.; Abramov, O.; Clifford, S. M.; Kring, D. A.; Lasue, J.; McGovern, P. J.; Treiman, A. H.; Wittmann, A.] Lunar & Planetary Inst, USRA, Houston, TX 77058 USA.
[Allen, C. C.] NASA JSC, ARES, Houston, TX 77058 USA.
[Bridges, J. C.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England.
[Filiberto, J.] So Illinois Univ, Geol Dept MC 4234, Carbondale, IL 62901 USA.
[Lasue, J.; Wiens, R. C.] Los Alamos Natl Lab, Space Remote Sensing, Los Alamos, NM 87545 USA.
[Newsom, H. E.; Vaniman, D. T.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Newsom, H. E.] Univ New Mexico, Dept Earth & Planetary Sci MSCO3 2050, Albuquerque, NM 87131 USA.
[Vaniman, D. T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Schwenzer, S. P.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Abramov, O.] US Geol Survey, Astrogeol Res Program, Flagstaff, AZ 86001 USA.
[Lasue, J.] Univ Toulouse, Toulouse, France.
[Lasue, J.] UPS OMP, Toulouse, France.
[Lasue, J.] IRAP, Toulouse, France.
[Wittmann, A.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO USA.
RP Schwenzer, SP (reprint author), Lunar & Planetary Inst, USRA, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM schwenzer@lpi.usra.edu; carlton.c.allen@nasa.gov; j.bridges@le.ac.uk;
clifford@lpi.usra.edu; Filiberto@siu.edu; kring@lpi.usra.edu;
lasue@lanl.gov; mcgovern@lpi.usra.edu; newsom@unm.edu;
treiman@lpi.usra.edu; dvaniman@psi.edu; rwiens@lanl.gov;
wittmann@levee.wustl.edu
OI Schwenzer, Susanne Petra/0000-0002-9608-0759; McGovern,
Patrick/0000-0001-9647-3096
FU National Aeronautics and Space Administration (NASA) Mars Fundamental
Research grants [NNX07AK42G, NNX09AL25G]; NASA MDAP grant [NNX09AI42G];
NASA Planetary Geology and Geophysics grant [NNH07DA001N]; NASA Mars
Science Laboratory project; NASA Astrobiology Institute fellowship
through the NASA Postdoctoral programme
FX This work was supported, in part, by National Aeronautics and Space
Administration (NASA) Mars Fundamental Research grants NNX07AK42G
(D.A.K. and S.P.S.) and NNX09AL25G (A.H.T. and J.F.); by NASA MDAP grant
number NNX09AI42G (P.J.M.); and by NASA Planetary Geology and Geophysics
grant NNH07DA001N (H.E.N.). The NASA Mars Science Laboratory project
supported R.C.W. and D.V., while a NASA Astrobiology Institute
fellowship awarded to O.A. through the NASA Postdoctoral programme
supported his work. We thank Charles Cockell and Nathalie Cabrol for
discussions that improved earlier versions of the manuscript. This is
Lunar and Planetary Institute (LPI) contribution 1626.
NR 97
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP
PY 2012
VL 70
IS 1
BP 84
EP 95
DI 10.1016/j.pss.2012.05.014
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 000LD
UT WOS:000308386900008
ER
PT J
AU Fairen, AG
Davila, AF
Schulze-Makuch, D
Rodriguez, JAP
McKay, CP
AF Fairen, Alberto G.
Davila, Alfonso F.
Schulze-Makuch, Dirk
Rodriguez, J. Alexis P.
McKay, Christopher P.
TI Glacial paleoenvironments on Mars revealed by the paucity of hydrated
silicates in the Noachian crust of the Northern Lowlands
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Phyllosilicates; Northern lowlands; Mars ocean
ID IMPACT CRATERS; SEDIMENTATION; PLAINS; OCEANS; ICE; PHYLLOSILICATES;
BASIN; ENVIRONMENT; EVOLUTION; CLIMATE
AB Hydrated silicates occur widespread in thousands of locations in the Martian Noachian-aged southern highlands. If an ocean existed on the northern lowlands of Mars during the Noachian, phyllosilicates are likewise expected to be present in the primeval crust of the Martian plains, since on Earth they are common products of continental fluvial transportation and oceanic sedimentation. Here we analyze data from spaceborne imaging spectrometers searching for Noachian Mg/Al-phyllosilicates in 198 impact craters in the northern lowlands of Mars, as impact-excavated materials have already been demonstrated as qualifying samples of preexisting subsurface deposits. Our results indicate that only 15 impact craters in the Martian lowlands show evidence of excavated Mg/Al-phyllosilicates (< 10%, consistent with previous estimates). We have also analyzed 88 craters in the highlands region located between -1000 and -3000 m, and in this case the number of craters showing excavated Mg/Al-phyllosilicates was 64 (> 70%). Therefore, hydrated silicates form a mineralogical dichotomy noticeable in the ancient Noachian crust on a global scale. This is indicative of little or no significant fluvial transportation of phyllosilicate-rich, southern highland materials into the northern basins. But the Noachian phyllosilicate-rich terrains in the southern highlands are heavily dissected by similar to 80,000 valley networks, revealing sustained surface runoff expected to be efficient at remobilizing sediments into the northern plains. The presence of widespread ice masses rimming cold glacial Noachian oceans is a plausible explanation for the lack of large-scale phyllosilicate minerals in the primeval basement of the lowlands of Mars. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Fairen, Alberto G.; Davila, Alfonso F.; McKay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Fairen, Alberto G.; Davila, Alfonso F.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA.
[Schulze-Makuch, Dirk] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99163 USA.
[Rodriguez, J. Alexis P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Fairen, AG (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
EM alberto.g.fairen@nasa.gov
RI Davila, Alfonso/A-2198-2013;
OI Davila, Alfonso/0000-0002-0977-9909; Schulze-Makuch,
Dirk/0000-0002-1923-9746
NR 53
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP
PY 2012
VL 70
IS 1
BP 126
EP 133
DI 10.1016/j.pss.2012.05.009
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 000LD
UT WOS:000308386900012
ER
PT J
AU Goetz, W
Hecht, MH
Hviid, SF
Madsen, MB
Pike, WT
Staufer, U
Velbel, MA
Harrit, NH
Zych, E
Edgett, KS
AF Goetz, W.
Hecht, M. H.
Hviid, S. F.
Madsen, M. B.
Pike, W. T.
Staufer, U.
Velbel, M. A.
Harrit, N. H.
Zych, E.
Edgett, K. S.
TI Search for ultraviolet luminescence of soil particles at the Phoenix
landing site, Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Soil particles; UV-excited luminescence; Phoenix; Optical
microscope (OM); Mars hand lens imager (MAHLI)
ID FLUORESCENCE; DEPOSITS; SILICA
AB The Optical Microscope (OM) on the Phoenix Mars lander (operated from May through October 2008) was used to search for visible-wavelength luminescence of soil particles excited by ultraviolet (UV) illumination (lambda = 360-390 nm). No luminescent particles were found, with the possible exception of a few potentially luminescent features comprising about 0.02% of the total soil volume. The luminescence quantum efficiency of bulk soil as well as individual soil particles at the Phoenix site is constrained to less than 0.04%. A similar UV experiment will be performed by the Mars Hand Lens Imager (MAHLI) on the upcoming Mars Science Laboratory (MSL) mission. We compare OM and MAHLI UV experiments to each other and suggest a strategy to search for UV-excited luminescence with MAHLI. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Goetz, W.; Hviid, S. F.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Hecht, M. H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Pike, W. T.] Univ London Imperial Coll Sci Technol & Med, Dept Elect & Elect Engn, London SW7 2AZ, England.
[Staufer, U.] Delft Univ Technol, Micro & Nano Engn Lab, Delft, Netherlands.
[Velbel, M. A.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA.
[Harrit, N. H.] Univ Copenhagen, Dept Chem, Nano Sci Ctr, DK-2100 Copenhagen, Denmark.
[Zych, E.] Univ Wroclaw, Fac Chem, PL-50138 Wroclaw, Poland.
[Edgett, K. S.] Malin Space Sci Syst, San Diego, CA USA.
RP Goetz, W (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
EM goetz@mps.mpg.de
RI Madsen, Morten/D-2082-2011; Staufer, Urs/J-6866-2016;
OI Madsen, Morten/0000-0001-8909-5111; Staufer, Urs/0000-0002-3519-6467;
Edgett, Kenneth/0000-0001-7197-5751
FU Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR) [50 QM 0602]; UK
Science and Technology Facilities Council; Wolferman Nageli Foundation;
NASA/JPL; Danish Research Agency; Lundbeck Foundation
FX This research was supported in part by Deutsches Zentrum fur Luft- und
Raumfahrt e.V. (DLR) grant 50 QM 0602, the UK Science and Technology
Facilities Council, the Wolferman Nageli Foundation, and NASA/JPL. M.B.
Madsen acknowledges support from the Danish Research Agency and from the
Lundbeck Foundation. The manuscript was improved by thoughtful comments
from Jeffrey R. Johnson, Johns Hopkins University, Applied Physics
Laboratory.
NR 24
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP
PY 2012
VL 70
IS 1
BP 134
EP 147
DI 10.1016/j.pss.2012.05.002
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 000LD
UT WOS:000308386900013
ER
PT J
AU Meyer, M
AF Meyer, Michael
TI Foreword: Mars Science Laboratory, the First Astrobiology Mission to
Mars Since Viking
SO SPACE SCIENCE REVIEWS
LA English
DT Editorial Material
C1 NASA Headquarters, Washington, DC USA.
RP Meyer, M (reprint author), NASA Headquarters, Washington, DC USA.
EM Michael.A.Meyer@nasa.gov
NR 0
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 3
EP 4
DI 10.1007/s11214-012-9927-8
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500002
ER
PT J
AU Grotzinger, JP
Crisp, J
Vasavada, AR
Anderson, RC
Baker, CJ
Barry, R
Blake, DF
Conrad, P
Edgett, KS
Ferdowski, B
Gellert, R
Gilbert, JB
Golombek, M
Gomez-Elvira, J
Hassler, DM
Jandura, L
Litvak, M
Mahaffy, P
Maki, J
Meyer, M
Malin, MC
Mitrofanov, I
Simmonds, JJ
Vaniman, D
Welch, RV
Wiens, RC
AF Grotzinger, John P.
Crisp, Joy
Vasavada, Ashwin R.
Anderson, Robert C.
Baker, Charles J.
Barry, Robert
Blake, David F.
Conrad, Pamela
Edgett, Kenneth S.
Ferdowski, Bobak
Gellert, Ralf
Gilbert, John B.
Golombek, Matt
Gomez-Elvira, Javier
Hassler, Donald M.
Jandura, Louise
Litvak, Maxim
Mahaffy, Paul
Maki, Justin
Meyer, Michael
Malin, Michael C.
Mitrofanov, Igor
Simmonds, John J.
Vaniman, David
Welch, Richard V.
Wiens, Roger C.
TI Mars Science Laboratory Mission and Science Investigation
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Curiosity; Rover; Gale; Mount Sharp
ID X-RAY SPECTROMETER; SEDIMENTARY-ROCKS; EVOLUTION; MINERALS; METHANE;
SURFACE; ORIGIN; LIFE
AB Scheduled to land in August of 2012, the Mars Science Laboratory (MSL) Mission was initiated to explore the habitability of Mars. This includes both modern environments as well as ancient environments recorded by the stratigraphic rock record preserved at the Gale crater landing site. The Curiosity rover has a designed lifetime of at least one Mars year (similar to 23 months), and drive capability of at least 20 km. Curiosity's science payload was specifically assembled to assess habitability and includes a gas chromatograph-mass spectrometer and gas analyzer that will search for organic carbon in rocks, regolith fines, and the atmosphere (SAM instrument); an x-ray diffractometer that will determine mineralogical diversity (CheMin instrument); focusable cameras that can image landscapes and rock/regolith textures in natural color (MAHLI, MARDI, and Mastcam instruments); an alpha-particle x-ray spectrometer for in situ determination of rock and soil chemistry (APXS instrument); a laser-induced breakdown spectrometer to remotely sense the chemical composition of rocks and minerals (ChemCam instrument); an active neutron spectrometer designed to search for water in rocks/regolith (DAN instrument); a weather station to measure modern-day environmental variables (REMS instrument); and a sensor designed for continuous monitoring of background solar and cosmic radiation (RAD instrument). The various payload elements will work together to detect and study potential sampling targets with remote and in situ measurements; to acquire samples of rock, soil, and atmosphere and analyze them in onboard analytical instruments; and to observe the environment around the rover.
The 155-km diameter Gale crater was chosen as Curiosity's field site based on several attributes: an interior mountain of ancient flat-lying strata extending almost 5 km above the elevation of the landing site; the lower few hundred meters of the mountain show a progression with relative age from clay-bearing to sulfate-bearing strata, separated by an unconformity from overlying likely anhydrous strata; the landing ellipse is characterized by a mixture of alluvial fan and high thermal inertia/high albedo stratified deposits; and a number of stratigraphically/geomorphically distinct fluvial features. Samples of the crater wall and rim rock, and more recent to currently active surface materials also may be studied. Gale has a well-defined regional context and strong evidence for a progression through multiple potentially habitable environments. These environments are represented by a stratigraphic record of extraordinary extent, and insure preservation of a rich record of the environmental history of early Mars. The interior mountain of Gale Crater has been informally designated at Mount Sharp, in honor of the pioneering planetary scientist Robert Sharp.
The major subsystems of the MSL Project consist of a single rover (with science payload), a Multi-Mission Radioisotope Thermoelectric Generator, an Earth-Mars cruise stage, an entry, descent, and landing system, a launch vehicle, and the mission operations and ground data systems. The primary communication path for downlink is relay through the Mars Reconnaissance Orbiter. The primary path for uplink to the rover is Direct-from-Earth. The secondary paths for downlink are Direct-to-Earth and relay through the Mars Odyssey orbiter.
Curiosity is a scaled version of the 6-wheel drive, 4-wheel steering, rocker bogie system from the Mars Exploration Rovers (MER) Spirit and Opportunity and the Mars Pathfinder Sojourner. Like Spirit and Opportunity, Curiosity offers three primary modes of navigation: blind-drive, visual odometry, and visual odometry with hazard avoidance. Creation of terrain maps based on HiRISE (High Resolution Imaging Science Experiment) and other remote sensing data were used to conduct simulated driving with Curiosity in these various modes, and allowed selection of the Gale crater landing site which requires climbing the base of a mountain to achieve its primary science goals.
The Sample Acquisition, Processing, and Handling (SA/SPaH) subsystem is responsible for the acquisition of rock and soil samples from the Martian surface and the processing of these samples into fine particles that are then distributed to the analytical science instruments. The SA/SPaH subsystem is also responsible for the placement of the two contact instruments (APXS, MAHLI) on rock and soil targets. SA/SPaH consists of a robotic arm and turret-mounted devices on the end of the arm, which include a drill, brush, soil scoop, sample processing device, and the mechanical and electrical interfaces to the two contact science instruments. SA/SPaH also includes drill bit boxes, the organic check material, and an observation tray, which are all mounted on the front of the rover, and inlet cover mechanisms that are placed over the SAM and CheMin solid sample inlet tubes on the rover top deck.
C1 [Grotzinger, John P.; Crisp, Joy; Vasavada, Ashwin R.; Anderson, Robert C.; Baker, Charles J.; Barry, Robert; Ferdowski, Bobak; Gilbert, John B.; Golombek, Matt; Jandura, Louise; Maki, Justin; Simmonds, John J.; Welch, Richard V.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Blake, David F.] NASA, Ames Res Ctr, Moffett Field, CA USA.
[Conrad, Pamela; Mahaffy, Paul] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Edgett, Kenneth S.; Malin, Michael C.] Malin Space Sci Syst, San Diego, CA USA.
[Gellert, Ralf] Univ Guelph, Guelph, ON N1G 2W1, Canada.
[Gomez-Elvira, Javier] Ctr Astrobiolo CSIC INTA, Madrid, Spain.
[Hassler, Donald M.] SW Res Inst, Boulder, CO USA.
[Litvak, Maxim; Mitrofanov, Igor] Space Res Inst IKI, Moscow, Russia.
[Meyer, Michael] NASA Headquarters, Washington, DC USA.
[Vaniman, David] Planetary Sci Inst, Houston, TX USA.
[Wiens, Roger C.] Los Alamos Natl Lab, Los Alamos, NM USA.
RP Grotzinger, JP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM grotz@gps.caltech.edu
RI Gomez-Elvira, Javier/K-5829-2014; Crisp, Joy/H-8287-2016;
OI Gomez-Elvira, Javier/0000-0002-9068-9846; Crisp,
Joy/0000-0002-3202-4416; Edgett, Kenneth/0000-0001-7197-5751
NR 39
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 5
EP 56
DI 10.1007/s11214-012-9892-2
PG 52
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500003
ER
PT J
AU Anderson, RC
Jandura, L
Okon, AB
Sunshine, D
Roumeliotis, C
Beegle, LW
Hurowitz, J
Kennedy, B
Limonadi, D
McCloskey, S
Robinson, M
Seybold, C
Brown, K
AF Anderson, R. C.
Jandura, L.
Okon, A. B.
Sunshine, D.
Roumeliotis, C.
Beegle, L. W.
Hurowitz, J.
Kennedy, B.
Limonadi, D.
McCloskey, S.
Robinson, M.
Seybold, C.
Brown, K.
TI Collecting Samples in Gale Crater, Mars; an Overview of the Mars Science
Laboratory Sample Acquisition, Sample Processing and Handling System
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars science laboratory; Sample acquisition; Sample processing and
handling system
AB The Mars Science Laboratory Mission (MSL), scheduled to land on Mars in the summer of 2012, consists of a rover and a scientific payload designed to identify and assess the habitability, geological, and environmental histories of Gale crater. Unraveling the geologic history of the region and providing an assessment of present and past habitability requires an evaluation of the physical and chemical characteristics of the landing site; this includes providing an in-depth examination of the chemical and physical properties of Martian regolith and rocks. The MSL Sample Acquisition, Processing, and Handling (SA/SPaH) subsystem will be the first in-situ system designed to acquire interior rock and soil samples from Martian surface materials. These samples are processed and separated into fine particles and distributed to two onboard analytical science instruments SAM (Sample Analysis at Mars Instrument Suite) and CheMin (Chemistry and Mineralogy) or to a sample analysis tray for visual inspection. The SA/SPaH subsystem is also responsible for the placement of the two contact instruments, Alpha Particle X-Ray Spectrometer (APXS), and the Mars Hand Lens Imager (MAHLI), on rock and soil targets. Finally, there is a Dust Removal Tool (DRT) to remove dust particles from rock surfaces for subsequent analysis by the contact and or mast mounted instruments (e.g. Mast Cameras (MastCam) and the Chemistry and Micro-Imaging instruments (ChemCam)).
C1 [Anderson, R. C.; Jandura, L.; Okon, A. B.; Sunshine, D.; Roumeliotis, C.; Beegle, L. W.; Hurowitz, J.; Kennedy, B.; Limonadi, D.; McCloskey, S.; Robinson, M.; Seybold, C.; Brown, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Anderson, RC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 264-640, Pasadena, CA 91109 USA.
EM robert.c.anderson@jpl.nasa.gov
NR 7
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U1 3
U2 42
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 57
EP 75
DI 10.1007/s11214-012-9898-9
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500004
ER
PT J
AU Maki, J
Thiessen, D
Pourangi, A
Kobzeff, P
Litwin, T
Scherr, L
Elliott, S
Dingizian, A
Maimone, M
AF Maki, J.
Thiessen, D.
Pourangi, A.
Kobzeff, P.
Litwin, T.
Scherr, L.
Elliott, S.
Dingizian, A.
Maimone, M.
TI The Mars Science Laboratory Engineering Cameras
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Cameras; Rovers; Mars Science Laboratory; Remote Sensing;
Instruments; Imaging systems; Planetary missions
ID STEREO
AB NASA's Mars Science Laboratory (MSL) Rover is equipped with a set of 12 engineering cameras. These cameras are build-to-print copies of the Mars Exploration Rover cameras described in Maki et al. (J. Geophys. Res. 108(E12): 8071, 2003). Images returned from the engineering cameras will be used to navigate the rover on the Martian surface, deploy the rover robotic arm, and ingest samples into the rover sample processing system. The Navigation cameras (Navcams) are mounted to a pan/tilt mast and have a 45-degree square field of view (FOV) with a pixel scale of 0.82 mrad/pixel. The Hazard Avoidance Cameras (Hazcams) are body-mounted to the rover chassis in the front and rear of the vehicle and have a 124-degree square FOV with a pixel scale of 2.1 mrad/pixel. All of the cameras utilize a 1024x1024 pixel detector and red/near IR bandpass filters centered at 650 nm. The MSL engineering cameras are grouped into two sets of six: one set of cameras is connected to rover computer "A" and the other set is connected to rover computer "B". The Navcams and Front Hazcams each provide similar views from either computer. The Rear Hazcams provide different views from the two computers due to the different mounting locations of the "A" and "B" Rear Hazcams. This paper provides a brief description of the engineering camera properties, the locations of the cameras on the vehicle, and camera usage for surface operations.
C1 [Maki, J.; Thiessen, D.; Pourangi, A.; Kobzeff, P.; Litwin, T.; Scherr, L.; Elliott, S.; Dingizian, A.; Maimone, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Maki, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 264-630, Pasadena, CA 91109 USA.
EM Justin.N.Maki@jpl.nasa.gov
NR 13
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 77
EP 93
DI 10.1007/s11214-012-9882-4
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500005
ER
PT J
AU Maurice, S
Wiens, RC
Saccoccio, M
Barraclough, B
Gasnault, O
Forni, O
Mangold, N
Baratoux, D
Bender, S
Berger, G
Bernardin, J
Berthe, M
Bridges, N
Blaney, D
Bouye, M
Cais, P
Clark, B
Clegg, S
Cousin, A
Cremers, D
Cros, A
DeFlores, L
Derycke, C
Dingler, B
Dromart, G
Dubois, B
Dupieux, M
Durand, E
d'Uston, L
Fabre, C
Faure, B
Gaboriaud, A
Gharsa, T
Herkenhoff, K
Kan, E
Kirkland, L
Kouach, D
Lacour, JL
Langevin, Y
Lasue, J
Le Mouelic, S
Lescure, M
Lewin, E
Limonadi, D
Manhes, G
Mauchien, P
McKay, C
Meslin, PY
Michel, Y
Miller, E
Newsom, HE
Orttner, G
Paillet, A
Pares, L
Parot, Y
Perez, R
Pinet, P
Poitrasson, F
Quertier, B
Salle, B
Sotin, C
Sautter, V
Seran, H
Simmonds, JJ
Sirven, JB
Stiglich, R
Striebig, N
Thocaven, JJ
Toplis, MJ
Vaniman, D
AF Maurice, S.
Wiens, R. C.
Saccoccio, M.
Barraclough, B.
Gasnault, O.
Forni, O.
Mangold, N.
Baratoux, D.
Bender, S.
Berger, G.
Bernardin, J.
Berthe, M.
Bridges, N.
Blaney, D.
Bouye, M.
Cais, P.
Clark, B.
Clegg, S.
Cousin, A.
Cremers, D.
Cros, A.
DeFlores, L.
Derycke, C.
Dingler, B.
Dromart, G.
Dubois, B.
Dupieux, M.
Durand, E.
d'Uston, L.
Fabre, C.
Faure, B.
Gaboriaud, A.
Gharsa, T.
Herkenhoff, K.
Kan, E.
Kirkland, L.
Kouach, D.
Lacour, J. -L.
Langevin, Y.
Lasue, J.
Le Mouelic, S.
Lescure, M.
Lewin, E.
Limonadi, D.
Manhes, G.
Mauchien, P.
McKay, C.
Meslin, P. -Y.
Michel, Y.
Miller, E.
Newsom, H. E.
Orttner, G.
Paillet, A.
Pares, L.
Parot, Y.
Perez, R.
Pinet, P.
Poitrasson, F.
Quertier, B.
Salle, B.
Sotin, C.
Sautter, V.
Seran, H.
Simmonds, J. J.
Sirven, J. -B.
Stiglich, R.
Striebig, N.
Thocaven, J. -J.
Toplis, M. J.
Vaniman, D.
TI The ChemCam Instrument Suite on the Mars Science Laboratory (MSL) Rover:
Science Objectives and Mast Unit Description
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Spectroscopy; LIBS; Instruments; Planetary surfaces; Chemical
composition
ID INDUCED BREAKDOWN SPECTROSCOPY; X-RAY SPECTROMETER; MERIDIANI-PLANUM;
PATHFINDER SITE; BOUNCE ROCK; SOILS; CHEMISTRY; DEPOSITS; WATER;
SHERGOTTITE
AB ChemCam is a remote sensing instrument suite on board the "Curiosity" rover (NASA) that uses Laser-Induced Breakdown Spectroscopy (LIBS) to provide the elemental composition of soils and rocks at the surface of Mars from a distance of 1.3 to 7 m, and a telescopic imager to return high resolution context and micro-images at distances greater than 1.16 m. We describe five analytical capabilities: rock classification, quantitative composition, depth profiling, context imaging, and passive spectroscopy. They serve as a toolbox to address most of the science questions at Gale crater. ChemCam consists of a Mast-Unit (laser, telescope, camera, and electronics) and a Body-Unit (spectrometers, digital processing unit, and optical demultiplexer), which are connected by an optical fiber and an electrical interface. We then report on the development, integration, and testing of the Mast-Unit, and summarize some key characteristics of ChemCam. This confirmed that nominal or better than nominal performances were achieved for critical parameters, in particular power density (> 1 GW/cm(2)). The analysis spot diameter varies from 350 mu m at 2 m to 550 mu m at 7 m distance. For remote imaging, the camera field of view is 20 mrad for 1024x1024 pixels. Field tests demonstrated that the resolution (similar to 90 mu rad) made it possible to identify laser shots on a wide variety of images. This is sufficient for visualizing laser shot pits and textures of rocks and soils. An auto-exposure capability optimizes the dynamical range of the images. Dedicated hardware and software focus the telescope, with precision that is appropriate for the LIBS and imaging depths-of-field. The light emitted by the plasma is collected and sent to the Body-Unit via a 6 m optical fiber. The companion to this paper (Wiens et al. this issue) reports on the development of the Body-Unit, on the analysis of the emitted light, and on the good match between instrument performance and science specifications.
C1 [Maurice, S.; Gasnault, O.; Forni, O.; Baratoux, D.; Berger, G.; Cousin, A.; Cros, A.; Dupieux, M.; d'Uston, L.; Gharsa, T.; Lasue, J.; Meslin, P. -Y.; Orttner, G.; Pares, L.; Parot, Y.; Pinet, P.; Salle, B.; Seran, H.; Thocaven, J. -J.; Toplis, M. J.] Univ Toulouse 3, CNRS, Inst Rech Astrophys & Planetol, Observ Midi Pyrenees, F-31062 Toulouse, France.
[Wiens, R. C.; Barraclough, B.; Bender, S.; Bernardin, J.; Clegg, S.; Dingler, B.; Lasue, J.; Stiglich, R.; Vaniman, D.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Saccoccio, M.; Faure, B.; Gaboriaud, A.; Michel, Y.; Paillet, A.; Perez, R.] Ctr Natl Etud Spatiales, F-31055 Toulouse, France.
[Mangold, N.; Le Mouelic, S.; Sotin, C.] Univ Nantes, CNRS, Lab Planetol & Geodynam, Nantes, France.
[Berthe, M.; Langevin, Y.] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France.
[Berthe, M.; Langevin, Y.] CNRS, F-91405 Orsay, France.
[Bridges, N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Blaney, D.; DeFlores, L.; Kan, E.; Limonadi, D.; Miller, E.; Sotin, C.; Simmonds, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bouye, M.; Dubois, B.; Kouach, D.; Striebig, N.] Observ Midi Pyrenees, Grp Instrumentat Sci, F-31400 Toulouse, France.
[Cais, P.; Quertier, B.] Univ Bordeaux, CNRS, Lab Astrophys Bordeaux, Floirac, France.
[Clark, B.] Space Sci Inst, Boulder, CO USA.
[Cremers, D.] Appl Res Associates, Albuquerque, NM USA.
[Derycke, C.; Durand, E.] Thales Optron Sa, Elancourt, France.
[Dromart, G.] Univ Lyon, Lab Geol Lyon, Ecole Normal Super Lyon, Lyon, France.
[Fabre, C.] Univ Lorraine, CNRS, Vandoeuvre Les Nancy, France.
[Herkenhoff, K.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Kirkland, L.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Lacour, J. -L.; Mauchien, P.; Salle, B.; Sirven, J. -B.] CEA, DEN, Dept Phys Chem, Gif Sur Yvette, France.
[Lewin, E.] Univ Grenoble 1, Inst Sci Terre, Grenoble, France.
[Lewin, E.] CNRS, Grenoble, France.
[Manhes, G.] Inst Phys Globe, Paris, France.
[McKay, C.] NASA, Ames Res Ctr, Mountain View, CA USA.
[Newsom, H. E.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Lescure, M.] CNRS, Lab Anal & Architecture Syst, Toulouse, France.
[Sautter, V.] Museum Natl Hist Nat, CNRS, Lab Mineral & Cosmochim, Paris, France.
[Vaniman, D.] Planetary Sci Inst, Tucson, AZ USA.
RP Maurice, S (reprint author), Univ Toulouse 3, CNRS, Inst Rech Astrophys & Planetol, Observ Midi Pyrenees, F-31062 Toulouse, France.
EM sylvestre.maurice@irap.omp.eu
RI Cecile, FABRE/B-5827-2012; Baratoux, David/H-6006-2012; Sirven,
Jean-Baptiste/H-5782-2013; Gasnault, Olivier/F-4327-2010; BERGER,
Gilles/F-7118-2016; LEWIN, Eric/F-1451-2017;
OI Baratoux, David/0000-0002-1785-5262; Sirven,
Jean-Baptiste/0000-0002-5523-6809; Clegg, Sam/0000-0002-0338-0948;
Gasnault, Olivier/0000-0002-6979-9012; Forni,
Olivier/0000-0001-6772-9689
FU France by the French Space Agency (CNES); Centre National de la
Recherche Scientifique (CNRS); NASA's Mars Program Office
FX This work was supported in France by the French Space Agency (CNES), the
Centre National de la Recherche Scientifique (CNRS), and many institutes
and universities across the country. It has benefitted from the
continuous support of the Observatoire Midi-Pyrenees (OMP) and its
director B. Dupre, where the Institut de Recherche en Astrophysique et
Planetologie (IRAP), the laboratory responsible of the delivery of
ChemCam Mast-Unit is located. Collaboration by colleagues in the US was
funded by NASA's Mars Program Office.
NR 74
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 95
EP 166
DI 10.1007/s11214-012-9912-2
PG 72
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500006
ER
PT J
AU Wiens, RC
Maurice, S
Barraclough, B
Saccoccio, M
Barkley, WC
Bell, JF
Bender, S
Bernardin, J
Blaney, D
Blank, J
Bouye, M
Bridges, N
Bultman, N
Cais, P
Clanton, RC
Clark, B
Clegg, S
Cousin, A
Cremers, D
Cros, A
DeFlores, L
Delapp, D
Dingler, R
D'Uston, C
Dyar, MD
Elliott, T
Enemark, D
Fabre, C
Flores, M
Forni, O
Gasnault, O
Hale, T
Hays, C
Herkenhoff, K
Kan, E
Kirkland, L
Kouach, D
Landis, D
Langevin, Y
Lanza, N
LaRocca, F
Lasue, J
Latino, J
Limonadi, D
Lindensmith, C
Little, C
Mangold, N
Manhes, G
Mauchien, P
McKay, C
Miller, E
Mooney, J
Morris, RV
Morrison, L
Nelson, T
Newsom, H
Ollila, A
Ott, M
Pares, L
Perez, R
Poitrasson, F
Provost, C
Reiter, JW
Roberts, T
Romero, F
Sautter, V
Salazar, S
Simmonds, JJ
Stiglich, R
Storms, S
Striebig, N
Thocaven, JJ
Trujillo, T
Ulibarri, M
Vaniman, D
Warner, N
Waterbury, R
Whitaker, R
Witt, J
Wong-Swanson, B
AF Wiens, Roger C.
Maurice, Sylvestre
Barraclough, Bruce
Saccoccio, Muriel
Barkley, Walter C.
Bell, James F., III
Bender, Steve
Bernardin, John
Blaney, Diana
Blank, Jennifer
Bouye, Marc
Bridges, Nathan
Bultman, Nathan
Cais, Phillippe
Clanton, Robert C.
Clark, Benton
Clegg, Samuel
Cousin, Agnes
Cremers, David
Cros, Alain
DeFlores, Lauren
Delapp, Dorothea
Dingler, Robert
D'Uston, Claude
Dyar, M. Darby
Elliott, Tom
Enemark, Don
Fabre, Cecile
Flores, Mike
Forni, Olivier
Gasnault, Olivier
Hale, Thomas
Hays, Charles
Herkenhoff, Ken
Kan, Ed
Kirkland, Laurel
Kouach, Driss
Landis, David
Langevin, Yves
Lanza, Nina
LaRocca, Frank
Lasue, Jeremie
Latino, Joseph
Limonadi, Daniel
Lindensmith, Chris
Little, Cynthia
Mangold, Nicolas
Manhes, Gerard
Mauchien, Patrick
McKay, Christopher
Miller, Ed
Mooney, Joe
Morris, Richard V.
Morrison, Leland
Nelson, Tony
Newsom, Horton
Ollila, Ann
Ott, Melanie
Pares, Laurent
Perez, Rene
Poitrasson, Franck
Provost, Cheryl
Reiter, Joseph W.
Roberts, Tom
Romero, Frank
Sautter, Violaine
Salazar, Steven
Simmonds, John J.
Stiglich, Ralph
Storms, Steven
Striebig, Nicolas
Thocaven, Jean-Jacques
Trujillo, Tanner
Ulibarri, Mike
Vaniman, David
Warner, Noah
Waterbury, Rob
Whitaker, Robert
Witt, James
Wong-Swanson, Belinda
TI The ChemCam Instrument Suite on the Mars Science Laboratory (MSL) Rover:
Body Unit and Combined System Tests
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Laser induced breakdown spectroscopy; LIBS; RMI; Mars Science
Laboratory; MSL; Curiosity; Gale Crater; Laser plasma; ChemCam
ID INDUCED BREAKDOWN SPECTROSCOPY; PLIOCENE MACUSANI VOLCANICS; GEOLOGICAL
SAMPLES; RAMAN-SPECTROSCOPY; SE PERU; LIBS; GEOCHEMISTRY; SPECTROGRAPH;
REFLECTANCE; MINERALOGY
AB The ChemCam instrument suite on the Mars Science Laboratory (MSL) rover Curiosity provides remote compositional information using the first laser-induced breakdown spectrometer (LIBS) on a planetary mission, and provides sample texture and morphology data using a remote micro-imager (RMI). Overall, ChemCam supports MSL with five capabilities: remote classification of rock and soil characteristics; quantitative elemental compositions including light elements like hydrogen and some elements to which LIBS is uniquely sensitive (e.g., Li, Be, Rb, Sr, Ba); remote removal of surface dust and depth profiling through surface coatings; context imaging; and passive spectroscopy over the 240-905 nm range. ChemCam is built in two sections: The mast unit, consisting of a laser, telescope, RMI, and associated electronics, resides on the rover's mast, and is described in a companion paper. ChemCam's body unit, which is mounted in the body of the rover, comprises an optical demultiplexer, three spectrometers, detectors, their coolers, and associated electronics and data handling logic. Additional instrument components include a 6 m optical fiber which transfers the LIBS light from the telescope to the body unit, and a set of onboard calibration targets. ChemCam was integrated and tested at Los Alamos National Laboratory where it also underwent LIBS calibration with 69 geological standards prior to integration with the rover. Post-integration testing used coordinated mast and instrument commands, including LIBS line scans on rock targets during system-level thermal-vacuum tests. In this paper we describe the body unit, optical fiber, and calibration targets, and the assembly, testing, and verification of the instrument prior to launch.
C1 [Wiens, Roger C.; Barraclough, Bruce; Barkley, Walter C.; Bender, Steve; Bernardin, John; Bultman, Nathan; Clanton, Robert C.; Clegg, Samuel; Delapp, Dorothea; Dingler, Robert; Enemark, Don; Flores, Mike; Hale, Thomas; Lanza, Nina; Lasue, Jeremie; Latino, Joseph; Little, Cynthia; Morrison, Leland; Nelson, Tony; Romero, Frank; Salazar, Steven; Stiglich, Ralph; Storms, Steven; Trujillo, Tanner; Ulibarri, Mike; Vaniman, David; Whitaker, Robert; Witt, James] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Maurice, Sylvestre; Bouye, Marc; Cousin, Agnes; Cros, Alain; D'Uston, Claude; Forni, Olivier; Gasnault, Olivier; Kouach, Driss; Lasue, Jeremie; Pares, Laurent; Poitrasson, Franck; Striebig, Nicolas; Thocaven, Jean-Jacques] Univ Toulouse 3, UPS OMP, IRAP, F-31400 Toulouse, France.
[Maurice, Sylvestre; Bouye, Marc; Cousin, Agnes; D'Uston, Claude; Forni, Olivier; Gasnault, Olivier; Kouach, Driss; Lasue, Jeremie; Pares, Laurent; Poitrasson, Franck; Striebig, Nicolas; Thocaven, Jean-Jacques] CNRS, IRAP, F-31028 Toulouse 4, France.
[Saccoccio, Muriel; Perez, Rene] Ctr Natl Etud Spatiales, F-31055 Toulouse, France.
[Bell, James F., III; Hays, Charles] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Blaney, Diana; DeFlores, Lauren; Elliott, Tom; Kan, Ed; Limonadi, Daniel; Lindensmith, Chris; Miller, Ed; Reiter, Joseph W.; Roberts, Tom; Simmonds, John J.; Warner, Noah] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Blank, Jennifer] Bay Area Environm Res Inst, Sonoma, CA USA.
[Bridges, Nathan] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Cais, Phillippe] Univ Bordeaux, Lab Astrophys Bordeaux, F-33299 Bordeaux, France.
[Clark, Benton] Space Sci Inst, Boulder, CO USA.
[Cremers, David] Appl Res Associates, Albuquerque, NM USA.
[Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
[Fabre, Cecile] Univ Nancy, F-54506 Vandoeuvre Les Nancy, France.
[Herkenhoff, Ken] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Kirkland, Laurel] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Landis, David] Charles Stark Draper Lab, Tampa, FL USA.
[Langevin, Yves] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Lanza, Nina; Newsom, Horton; Ollila, Ann] Univ New Mexico, Albuquerque, NM 87131 USA.
[LaRocca, Frank; Ott, Melanie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mangold, Nicolas] Univ Nantes, CNRS, LPGN, UMR6112, Nantes, France.
[Manhes, Gerard] Inst Phys Globe, F-75252 Paris, France.
[Mauchien, Patrick] Commissariat Energie Atom & Energies Alternat, F-91191 Gif Sur Yvette, France.
[Blank, Jennifer; McKay, Christopher] NASA, Ames Res Ctr, Mountain View, CA USA.
[Mooney, Joe; Provost, Cheryl] CeramOptec Ind Inc, E Longmeadow, MA USA.
[Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Sautter, Violaine] Museum Natl Hist Nat, Lab Mineral, F-75005 Paris, France.
[Sautter, Violaine] Museum Natl Hist Nat, Cosmochim Museum, F-75005 Paris, France.
[Waterbury, Rob] Ocean Opt Inc, Dunedin, FL USA.
[Wong-Swanson, Belinda] Innov8 LLC, Santa Fe, NM USA.
[Barraclough, Bruce; Bender, Steve; Vaniman, David] Planetary Sci Inst, Tucson, AZ USA.
RP Wiens, RC (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA.
EM rwiens@lanl.gov
RI Cecile, FABRE/B-5827-2012; Gasnault, Olivier/F-4327-2010;
OI Gasnault, Olivier/0000-0002-6979-9012; Forni,
Olivier/0000-0001-6772-9689; Clegg, Sam/0000-0002-0338-0948
FU NASA Mars Program in the US; CNES in France; NASA
FX This work was supported by the NASA Mars Program in the US and CNES in
France. Pre-selection development of LIBS for planetary science was
supported in the US by grants from NASA's Mars Instrument Development
Program (MIDP). The ChemCam team wishes to thank the additional people
who supported the ChemCam program at various institutions, including
Thomas Liimatainen who fabricated the calibration target body.
Assistance at LANL by E. Michel, J. Salazar, R. D. Gurule, P. Archuleta,
A. Mezzacappa, L.-M. Nortier, L. Salazar, D. Mietz, E. Fenimore, B.
Dougherty, M. Fazio, and K. Saeger was greatly appreciated.
NR 54
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U2 84
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 167
EP 227
DI 10.1007/s11214-012-9902-4
PG 61
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500007
ER
PT J
AU Edgett, KS
Yingst, RA
Ravine, MA
Caplinger, MA
Maki, JN
Ghaemi, FT
Schaffner, J
Bell, JF
Edwards, LJ
Herkenhoff, KE
Heydari, E
Kah, LC
Lemmon, MT
Minitti, ME
Olson, TS
Parker, TJ
Rowland, SK
Schieber, J
Sullivan, RJ
Sumner, DY
Thomas, PC
Jensen, EH
Simmonds, JJ
Sengstacken, AJ
Willson, RG
Goetz, W
AF Edgett, Kenneth S.
Yingst, R. Aileen
Ravine, Michael A.
Caplinger, Michael A.
Maki, Justin N.
Ghaemi, F. Tony
Schaffner, Jacob A.
Bell, James F., III
Edwards, Laurence J.
Herkenhoff, Kenneth E.
Heydari, Ezat
Kah, Linda C.
Lemmon, Mark T.
Minitti, Michelle E.
Olson, Timothy S.
Parker, Timothy J.
Rowland, Scott K.
Schieber, Juergen
Sullivan, Robert J.
Sumner, Dawn Y.
Thomas, Peter C.
Jensen, Elsa H.
Simmonds, John J.
Sengstacken, Aaron J.
Willson, Reg G.
Goetz, Walter
TI Curiosity's Mars Hand Lens Imager (MAHLI) Investigation
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE MAHLI; Curiosity; Mars; Rover; Camera; Gale; Sediment
ID ROBOTIC ARM CAMERA; MERIDIANI-PLANUM; GUSEV CRATER; MICROSCOPIC IMAGER;
BURNS FORMATION; FOSSIL EVIDENCE; SPIRIT ROVER; LIFE; ROCKS; EARTH
AB The Mars Science Laboratory (MSL) Mars Hand Lens Imager (MAHLI) investigation will use a 2-megapixel color camera with a focusable macro lens aboard the rover, Curiosity, to investigate the stratigraphy and grain-scale texture, structure, mineralogy, and morphology of geologic materials in northwestern Gale crater. Of particular interest is the stratigraphic record of a similar to 5 km thick layered rock sequence exposed on the slopes of Aeolis Mons (also known as Mount Sharp). The instrument consists of three parts, a camera head mounted on the turret at the end of a robotic arm, an electronics and data storage assembly located inside the rover body, and a calibration target mounted on the robotic arm shoulder azimuth actuator housing. MAHLI can acquire in-focus images at working distances from similar to 2.1 cm to infinity. At the minimum working distance, image pixel scale is similar to 14 mu m per pixel and very coarse silt grains can be resolved. At the working distance of the Mars Exploration Rover Microscopic Imager cameras aboard Spirit and Opportunity, MAHLI's resolution is comparable at similar to 30 mu m per pixel. Onboard capabilities include autofocus, auto-exposure, sub-framing, video imaging, Bayer pattern color interpolation, lossy and lossless compression, focus merging of up to 8 focus stack images, white light and longwave ultraviolet (365 nm) illumination of nearby subjects, and 8 gigabytes of non-volatile memory data storage.
C1 [Edgett, Kenneth S.; Ravine, Michael A.; Caplinger, Michael A.; Schaffner, Jacob A.; Jensen, Elsa H.] Malin Space Sci Syst Inc, San Diego, CA 92191 USA.
[Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ USA.
[Maki, Justin N.; Parker, Timothy J.; Simmonds, John J.; Sengstacken, Aaron J.; Willson, Reg G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Ghaemi, F. Tony] Ghaemi Opt Engn, San Diego, CA USA.
[Bell, James F., III] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Edwards, Laurence J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Herkenhoff, Kenneth E.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Heydari, Ezat] Jackson State Univ, Jackson, MS USA.
[Kah, Linda C.] Univ Tennessee, Knoxville, TN USA.
[Lemmon, Mark T.] Texas A&M Univ, College Stn, TX USA.
[Minitti, Michelle E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Olson, Timothy S.] Salish Kootenai Coll, Pablo, MT USA.
[Rowland, Scott K.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Schieber, Juergen] Indiana Univ, Bloomington, IN USA.
[Sullivan, Robert J.; Thomas, Peter C.] Cornell Univ, Ithaca, NY USA.
[Sumner, Dawn Y.] Univ Calif Davis, Davis, CA 95616 USA.
[Goetz, Walter] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
RP Edgett, KS (reprint author), Malin Space Sci Syst Inc, POB 910148, San Diego, CA 92191 USA.
EM edgett@msss.com
RI Lemmon, Mark/E-9983-2010; Schieber, Juergen Schieber/A-3001-2013;
OI Lemmon, Mark/0000-0002-4504-5136; Edgett, Kenneth/0000-0001-7197-5751
FU JPL-Caltech [1269421, 1273887]; NASA [NAS7-03001, NMO710846]
FX The MSL MAHLI investigation is supported by USA taxpayers through NASA.
Specifically, the MAHLI team and MSSS developed the instrument and
investigation under subcontracts 1269421 and 1273887 in collaboration
with JPL-Caltech under NASA contracts NAS7-03001 and NMO710846.
JPL-Caltech manages MSL for NASA and part of this research was carried
out at JPL. Hundreds of people ultimately contributed to the development
of MAHLI and the capabilities to deliver and move the instrument around
Curiosity's field site on Mars. We heartily thank all of them, although
we regret we cannot name them all here. First and foremost, we thank our
spouses, partners and families for their support and sacrifices during
the >8 years since we first began working on MAHLI. In addition, we very
much thank: M. C. Malin, B. A. Cantor, K. D. Supulver, B. Hallet, W. E.
Dietrich, J.F. Cameron; the engineers at Alliance Spacesystems (now the
Space Division of MacDonald Dettwiler and Associates MDA Information
Systems): D. DiBiase, J. Laramee, B. Lindenfeld, R. Billing, H.
Aslanian, R. McKenzie, R. Gov, S. Dougherty, J. Baker, C. Corbin, T.
Cameron; MSSS engineering support from S. Brylow, P. Otjens, C. Martin,
H. Olawale, M. Clark, K. Schaffner, J. Tamayo; MSSS administrative
support: M. Mullenniex, L. Maze, D. Michna; MSSS instrument calibration
and ground data system support: S. McNair, B. M. Duston; MAHLI
operations development: L. V. Posiolova, M. Kennedy Wu, L. Lipkaman, B.
Nixon, R. Zimdar, B. Baker, J. Sandoval; MAHLI focus merge software
development by T. Lesperance; MSSS information technology and software
support from S. Davis; Spectra Systems and W. Lilly for donation of the
SpectraFluor Red pigment; D. T. Britt for production of the fluorescent
calibration target swatch; D. Szwabowski for design of the MAHLI
calibration target Ti plate; the MSL Project Scientists: J. P.
Grotzinger (2007-Present), E. Stolper (2005-2007), F. D. Palluconi
(2004-2005); the MSL Deputy Project Scientists: J. Crisp, A. R.
Vasavada; MSL Project Managers: P. Theisinger, R. Cook; the MSL Program
Scientist M. Meyer; Deputy Program Scientist M. Voytek; MSL SA/SPaH
support, particularly L. Jandura, R. B. Anderson and their colleagues;
JPL MSL robotic arm engineers M. Robinson, C. Collins, and colleagues;
JPL MSL development and testing personnel, including A. Thompson, J.
Samuels, D. Gruel, D. Limonadi, R. Heninger, B. Pavri, S. Howard, D.
Johnson, M. Johnson, and many others; instrument testing support at
Cubic Defense Applications: T. Le, K. Shannon; JPL MSL operations
planning: M. Watkins, N. Spanovich; L. Keely, D. Lees, and others at
NASA Ames for planning and analysis software development; the MAHLI
Preliminary Design Review Board: T. Fraschetti (chair), J. Baker, G.
Fraschetti, P. Wu, W. Harris, R. Kemski, W. Mateer, G. Reeves, F.
Vescelus, R. West, J. Johnson, P. Hardy; the MAHLI Critical Design
Review Board: T. Fraschetti (chair), G. Fraschetti, H. Kieffer, W.
Harris, C. Kingery, W. Mateer, G. Reeves, F. Vescelus, R. West, P.
Hardy, G. Kinsella; the MAHLI Instrument Delivery Review Board: T.
Fraschetti (chair), H. Kieffer, W. Harris, C. Kingery, W. Mateer, G.
Reeves, R. Paynter, A. Vasavada; the MAHLI Characterization and
Calibration independent review board: N. Izenberg, J. Johnson, K.
Klaasen, R. West. B. M. Duston, B. A. Cantor, T. J. Van Beek assisted
with refinement of the MAHLI motor count, working distance, pixel scale
relationships; B. A. Cantor assisted with the MRO MARCI figure. Finally,
we very much appreciate J. Blue, E. Lee, J. Richie, M.; Rosiek, and two
unidentified colleagues for their helpful suggestions stemming from
their reviews of the February 2012 version of this manuscript.
NR 71
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 259
EP 317
DI 10.1007/s11214-012-9910-4
PG 59
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500009
ER
PT J
AU Blake, D
Vaniman, D
Achilles, C
Anderson, R
Bish, D
Bristow, T
Chen, C
Chipera, S
Crisp, J
Des Marais, D
Downs, RT
Farmer, J
Feldman, S
Fonda, M
Gailhanou, M
Ma, HW
Ming, DW
Morris, RV
Sarrazin, P
Stolper, E
Treiman, A
Yen, A
AF Blake, David
Vaniman, David
Achilles, Cherie
Anderson, Robert
Bish, David
Bristow, Tom
Chen, Curtis
Chipera, Steve
Crisp, Joy
Des Marais, David
Downs, Robert T.
Farmer, Jack
Feldman, Sabrina
Fonda, Mark
Gailhanou, Marc
Ma, Hongwei
Ming, Doug W.
Morris, Richard V.
Sarrazin, Philippe
Stolper, Ed
Treiman, Allan
Yen, Albert
TI Characterization and Calibration of the CheMin Mineralogical Instrument
on Mars Science Laboratory
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE X-ray diffraction; Mineralogy; Mars habitability; Mars science
laboratory; Planetary science; Spacecraft instruments
ID METEORITE ALH84001; ROCKS; IDENTIFICATION; SPITSBERGEN; DIVERSITY;
CLIMATE
AB A principal goal of the Mars Science Laboratory (MSL) rover Curiosity is to identify and characterize past habitable environments on Mars. Determination of the mineralogical and chemical composition of Martian rocks and soils constrains their formation and alteration pathways, providing information on climate and habitability through time. The CheMin X-ray diffraction (XRD) and X-ray fluorescence (XRF) instrument on MSL will return accurate mineralogical identifications and quantitative phase abundances for scooped soil samples and drilled rock powders collected at Gale Crater during Curiosity's 1-Mars-year nominal mission. The instrument has a Co X-ray source and a cooled charge-coupled device (CCD) detector arranged in transmission geometry with the sample. CheMin's angular range of 5(a similar to) to 50(a similar to) 2 theta with < 0.35(a similar to) 2 theta resolution is sufficient to identify and quantify virtually all minerals. CheMin's XRF requirement was descoped for technical and budgetary reasons. However, X-ray energy discrimination is still required to separate Co K alpha from Co K beta and Fe K alpha photons. The X-ray energy-dispersive histograms (EDH) returned along with XRD for instrument evaluation should be useful in identifying elements Z > 13 that are contained in the sample. The CheMin XRD is equipped with internal chemical and mineralogical standards and 27 reusable sample cells with either Mylar(A (R)) or Kapton(A (R)) windows to accommodate acidic-to-basic environmental conditions. The CheMin flight model (FM) instrument will be calibrated utilizing analyses of common samples against a demonstration-model (DM) instrument and CheMin-like laboratory instruments. The samples include phyllosilicate and sulfate minerals that are expected at Gale crater on the basis of remote sensing observations.
C1 [Blake, David; Bristow, Tom; Des Marais, David] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Vaniman, David] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Achilles, Cherie] ESCG Hamilton Sundstrand, Houston, TX 77058 USA.
[Anderson, Robert; Chen, Curtis; Crisp, Joy; Feldman, Sabrina; Yen, Albert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bish, David; Ma, Hongwei] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Chipera, Steve] Chesapeake Energy Corp, Oklahoma City, OK 73118 USA.
[Downs, Robert T.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Farmer, Jack] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Fonda, Mark] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gailhanou, Marc] Fac Sci & Tech St Jerome, F-13397 Marseille 20, France.
[Ming, Doug W.; Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Sarrazin, Philippe] SETI Inst, Mountain View, CA 94043 USA.
[Stolper, Ed] CALTECH, Pasadena, CA 91125 USA.
[Treiman, Allan] Lunar & Planetary Inst, Houston, TX 77058 USA.
RP Blake, D (reprint author), NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM david.blake@nasa.gov
RI Gailhanou, Marc/F-8251-2014; Crisp, Joy/H-8287-2016
OI Gailhanou, Marc/0000-0002-7747-703X; Crisp, Joy/0000-0002-3202-4416
NR 52
TC 53
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U1 2
U2 45
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 341
EP 399
DI 10.1007/s11214-012-9905-1
PG 59
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500011
ER
PT J
AU Mahaffy, PR
Webster, CR
Cabane, M
Conrad, PG
Coll, P
Atreya, SK
Arvey, R
Barciniak, M
Benna, M
Bleacher, L
Brinckerhoff, WB
Eigenbrode, JL
Carignan, D
Cascia, M
Chalmers, RA
Dworkin, JP
Errigo, T
Everson, P
Franz, H
Farley, R
Feng, S
Frazier, G
Freissinet, C
Glavin, DP
Harpold, DN
Hawk, D
Holmes, V
Johnson, CS
Jones, A
Jordan, P
Kellogg, J
Lewis, J
Lyness, E
Malespin, CA
Martin, DK
Maurer, J
McAdam, AC
McLennan, D
Nolan, TJ
Noriega, M
Pavlov, AA
Prats, B
Raaen, E
Sheinman, O
Sheppard, D
Smith, J
Stern, JC
Tan, F
Trainer, M
Ming, DW
Morris, RV
Jones, J
Gundersen, C
Steele, A
Wray, J
Botta, O
Leshin, LA
Owen, T
Battel, S
Jakosky, BM
Manning, H
Squyres, S
Navarro-Gonzalez, R
McKay, CP
Raulin, F
Sternberg, R
Buch, A
Sorensen, P
Kline-Schoder, R
Coscia, D
Szopa, C
Teinturier, S
Baffes, C
Feldman, J
Flesch, G
Forouhar, S
Garcia, R
Keymeulen, D
Woodward, S
Block, BP
Arnett, K
Miller, R
Edmonson, C
Gorevan, S
Mumm, E
AF Mahaffy, Paul R.
Webster, Christopher R.
Cabane, Michel
Conrad, Pamela G.
Coll, Patrice
Atreya, Sushil K.
Arvey, Robert
Barciniak, Michael
Benna, Mehdi
Bleacher, Lora
Brinckerhoff, William B.
Eigenbrode, Jennifer L.
Carignan, Daniel
Cascia, Mark
Chalmers, Robert A.
Dworkin, Jason P.
Errigo, Therese
Everson, Paula
Franz, Heather
Farley, Rodger
Feng, Steven
Frazier, Gregory
Freissinet, Caroline
Glavin, Daniel P.
Harpold, Daniel N.
Hawk, Douglas
Holmes, Vincent
Johnson, Christopher S.
Jones, Andrea
Jordan, Patrick
Kellogg, James
Lewis, Jesse
Lyness, Eric
Malespin, Charles A.
Martin, David K.
Maurer, John
McAdam, Amy C.
McLennan, Douglas
Nolan, Thomas J.
Noriega, Marvin
Pavlov, Alexander A.
Prats, Benito
Raaen, Eric
Sheinman, Oren
Sheppard, David
Smith, James
Stern, Jennifer C.
Tan, Florence
Trainer, Melissa
Ming, Douglas W.
Morris, Richard V.
Jones, John
Gundersen, Cindy
Steele, Andrew
Wray, James
Botta, Oliver
Leshin, Laurie A.
Owen, Tobias
Battel, Steve
Jakosky, Bruce M.
Manning, Heidi
Squyres, Steven
Navarro-Gonzalez, Rafael
McKay, Christopher P.
Raulin, Francois
Sternberg, Robert
Buch, Arnaud
Sorensen, Paul
Kline-Schoder, Robert
Coscia, David
Szopa, Cyril
Teinturier, Samuel
Baffes, Curt
Feldman, Jason
Flesch, Greg
Forouhar, Siamak
Garcia, Ray
Keymeulen, Didier
Woodward, Steve
Block, Bruce P.
Arnett, Ken
Miller, Ryan
Edmonson, Charles
Gorevan, Stephen
Mumm, Erik
TI The Sample Analysis at Mars Investigation and Instrument Suite
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars, organic compounds; Volatiles; Isotopes; Evolved gas analysis; Gas
chromatography mass spectrometry; Noble gases; Habitability; Mars
Science Laboratory; Curiosity Rover; Gale crater
ID MARTIAN METEORITE ALH84001; VIKING BIOLOGY EXPERIMENTS; REFRACTORY
ORGANIC-MATTER; PHOENIX LANDING SITE; ALLAN HILLS 84001;
GAS-CHROMATOGRAPHY; ISOTOPIC COMPOSITION; SNC METEORITES;
THERMAL-DECOMPOSITION; OXIDANT ENHANCEMENT
AB The Sample Analysis at Mars (SAM) investigation of the Mars Science Laboratory (MSL) addresses the chemical and isotopic composition of the atmosphere and volatiles extracted from solid samples. The SAM investigation is designed to contribute substantially to the mission goal of quantitatively assessing the habitability of Mars as an essential step in the search for past or present life on Mars. SAM is a 40 kg instrument suite located in the interior of MSL's Curiosity rover. The SAM instruments are a quadrupole mass spectrometer, a tunable laser spectrometer, and a 6-column gas chromatograph all coupled through solid and gas processing systems to provide complementary information on the same samples. The SAM suite is able to measure a suite of light isotopes and to analyze volatiles directly from the atmosphere or thermally released from solid samples. In addition to measurements of simple inorganic compounds and noble gases SAM will conduct a sensitive search for organic compounds with either thermal or chemical extraction from sieved samples delivered by the sample processing system on the Curiosity rover's robotic arm.
C1 [Mahaffy, Paul R.; Conrad, Pamela G.; Arvey, Robert; Barciniak, Michael; Benna, Mehdi; Bleacher, Lora; Brinckerhoff, William B.; Eigenbrode, Jennifer L.; Carignan, Daniel; Cascia, Mark; Chalmers, Robert A.; Dworkin, Jason P.; Errigo, Therese; Everson, Paula; Franz, Heather; Farley, Rodger; Feng, Steven; Frazier, Gregory; Freissinet, Caroline; Glavin, Daniel P.; Harpold, Daniel N.; Hawk, Douglas; Holmes, Vincent; Johnson, Christopher S.; Jones, Andrea; Jordan, Patrick; Kellogg, James; Lewis, Jesse; Lyness, Eric; Malespin, Charles A.; Martin, David K.; Maurer, John; McAdam, Amy C.; McLennan, Douglas; Nolan, Thomas J.; Noriega, Marvin; Pavlov, Alexander A.; Prats, Benito; Raaen, Eric; Sheinman, Oren; Sheppard, David; Smith, James; Stern, Jennifer C.; Tan, Florence; Trainer, Melissa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Webster, Christopher R.; Baffes, Curt; Feldman, Jason; Flesch, Greg; Forouhar, Siamak; Garcia, Ray; Keymeulen, Didier; Woodward, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cabane, Michel; Coscia, David; Szopa, Cyril; Teinturier, Samuel] Univ Versailles St Quentin, Univ Paris 06, UPMC, CNRS,INSU,LATMOS IPSL, F-75005 Paris, France.
[Coll, Patrice] Univ Paris Est Creteil, CNRS, Inst Univ France, CMC,LISA, F-94010 Creteil, France.
[Atreya, Sushil K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Ming, Douglas W.; Morris, Richard V.; Jones, John] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Gundersen, Cindy] AMU Engn, Miami, FL 33156 USA.
[Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Wray, James] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Botta, Oliver] Swiss Space Off, Bern, Switzerland.
[Leshin, Laurie A.] Rensselaer Polytech Inst, Dept Earth & Environm Sci, Troy, NY 12180 USA.
[Owen, Tobias] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Battel, Steve] Battel Engn, Scottsdale, AZ 85253 USA.
[Jakosky, Bruce M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Manning, Heidi] Concordia Coll, Moorhead, MN 56562 USA.
[Squyres, Steven] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico.
[McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Raulin, Francois; Sternberg, Robert] Univ Paris 07, LISA, F-94010 Creteil, France.
[Raulin, Francois; Sternberg, Robert] CNRS, CMC, F-94010 Creteil, France.
[Buch, Arnaud] Ecole Cent Paris, Chatenay Malabry, France.
[Sorensen, Paul; Kline-Schoder, Robert] Creare Corp, Hanover, NH 03755 USA.
[Block, Bruce P.; Arnett, Ken; Miller, Ryan; Edmonson, Charles] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA.
[Gorevan, Stephen; Mumm, Erik] Honeybee Robotics Spacecraft Mech Corp, New York, NY 10001 USA.
RP Mahaffy, PR (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Paul.R.Mahaffy@nasa.gov
RI Gonzalez, Rafael/D-1748-2009; Steele, Andrew/A-3573-2013; Wray,
James/B-8457-2008; Pavlov, Alexander/F-3779-2012; Harpold,
Dan/I-3345-2013; freissinet, caroline/F-2431-2012; Brinckerhoff,
William/F-3453-2012; Stern, Jennifer/E-3135-2012; Glavin,
Daniel/D-6194-2012; szopa, cyril/C-6865-2015; Benna, Mehdi/F-3489-2012;
Dworkin, Jason/C-9417-2012
OI Wray, James/0000-0001-5559-2179; Pavlov, Alexander/0000-0001-8771-1646;
Brinckerhoff, William/0000-0001-5121-2634; Stern,
Jennifer/0000-0002-0162-8807; Glavin, Daniel/0000-0001-7779-7765; szopa,
cyril/0000-0002-0090-4056; Dworkin, Jason/0000-0002-3961-8997
FU JPL management; Centre National d'Etudes Spaciales; Science Mission
Directorate of the National Aeronautics and Space Administration
FX Support from the Mars Science Laboratory Payload Manager Jeff Simmonds
and the Project Science Team John Grotzinger, Joy Crisp, and Ashwin
Vasvada, the Program Scientist Michael Meyer, and the first Project
Scientist Edward Stolper is acknowledged. From the French Space Agency
CNES A. Gaboriaud for CNES CST engineering and for the CNES ground
segment Eric Lorigny. Contributions to the SAM science definition are
acknowledged from Wes Huntress, Robert Pepin, Wayne Kasprzak, Fred
Goesmann, Wadhwa Meenakshi, Edward Vicenzi, Kenneth Nealson, Audrey
Noblet, Carole Philippon, Loic Soldiani, Alain Person, Claude
Geffroy-Rodier, and Guy Israel. Special acknowledgement is given SAM
Co-investigator James Scott and science collaborator Gordon McKay who
both passed away during the SAM development. Helpful contributions to
analog studies were contributed by Brad Sutter and Doug Archer. In
addition to co-authors, numerous individuals contributed to the design,
fabrication, qualification, integration, test, and calibration of SAM.
These include James Odom, Irving Linares, Phillip Goodman, Mark Wolf,
Curt Cooper, Ray Bendt, Steven Cagiano, Yury Flom, Suong Le, John
Bishop, Mark McClendon, Roger Counts, Keith Corse, Joyce Manning, Greg
Hidrobo, Ryan Wilkinson, Rick Scott, Matthew Lefavor, George Winkert,
Norman Dobson, Nick Dobson, Mathew Lefavor, David Mcclaeb, Jerry
Hengemihle, Kiran Patel, Micah Johnson, Christa Budinoff, Ferzan Jaeger,
Joelle Cooperrider, Akif Ersahin, Charles Fleetwood, John Canham,
Rebecca Prats, Robert Kiwak, Anthony Sanders, Jamie Demick, Carol Lilly,
Lou Fetter, Bruce Meinhold, Christine Collins, Francesco Giacobbe, Amil
Mann, Mario Martins, Shawn McLeod, Carol Mosier, Daniel Powers, Brian
Rice, Cynthis Simmons, Ray Trunzo, Janelle Vorreiter, Kiel Davis, Jerri
Ji, Lee Carlson, Thomas Kennedy, Michael Rutberg, Marie-Sophie Clerc,
Jean-Jacques Correia, Alexandre Galic, Vincent Guerrini, Mustapha
Meftah, Christophe Montaron, Patrick Poinsignon, Curt Henry, Martin
Buehler, Steve Woodward, and Jean-Baptiste Rigal. Special
acknowledgement is given a valued Goddard colleague Robert Abell who
contributed greatly to the fabrication of critical SAM elements before
his death in 2008. During SAM integration with Curiosity Rover
significant support was provided by Richard Redick and Joseph Melko of
JPL. SAM-GC industrial partners included Air Liquide Advanced
Technologies, Comat Aerospace, ATERMES, Restek, and Varian Inc. (now
Agilent Technologies). Thanks to Ray Ardvison and Paul Niles for helpful
reviewer comments. Finally support from many individuals at NASA
Headquarters and both Goddard and JPL management is acknowledged with
special thanks to Orlando Figueroa, Charles Elachi, Doug McCuistion, Jim
Garvin, Anne Kinney, and Ed Weiler. The SAM GC was funded by the Centre
National d'Etudes Spaciales and the SAM Suite by the Science Mission
Directorate of the National Aeronautics and Space Administration.
NR 181
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 401
EP 478
DI 10.1007/s11214-012-9879-z
PG 78
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500012
ER
PT J
AU Conrad, PG
Eigenbrode, JL
Von der Heydt, MO
Mogensen, CT
Canham, J
Harpold, DN
Johnson, J
Errigo, T
Glavin, DP
Mahaffy, PR
AF Conrad, Pamela G.
Eigenbrode, Jennifer L.
Von der Heydt, Max O.
Mogensen, Claus T.
Canham, John
Harpold, Dan N.
Johnson, Joel
Errigo, Therese
Glavin, Daniel P.
Mahaffy, Paul R.
TI The Mars Science Laboratory Organic Check Material
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Mars science laboratory; MSL; SAM; Organic check material; OCM;
Contamination; Sample chain
ID GALE-CRATER
AB Mars Science Laboratory's Curiosity rover carries a set of five external verification standards in hermetically sealed containers that can be sampled as would be a Martian rock, by drilling and then portioning into the solid sample inlet of the Sample Analysis at Mars (SAM) suite. Each organic check material (OCM) canister contains a porous ceramic solid, which has been doped with a fluorinated hydrocarbon marker that can be detected by SAM. The purpose of the OCM is to serve as a verification tool for the organic cleanliness of those parts of the sample chain that cannot be cleaned other than by dilution, i.e., repeated sampling of Martian rock. SAM possesses internal calibrants for verification of both its performance and its internal cleanliness, and the OCM is not used for that purpose. Each OCM unit is designed for one use only, and the choice to do so will be made by the project science group (PSG).
C1 [Conrad, Pamela G.; Eigenbrode, Jennifer L.; Harpold, Dan N.; Errigo, Therese; Glavin, Daniel P.; Mahaffy, Paul R.] NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Von der Heydt, Max O.; Mogensen, Claus T.; Johnson, Joel] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Canham, John] ATK Space Syst Inc, Beltsville, MD USA.
RP Conrad, PG (reprint author), NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Code 699,Bldg 33,Rm C105,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Pamela.G.Conrad@nasa.gov
RI Harpold, Dan/I-3345-2013; Glavin, Daniel/D-6194-2012
OI Glavin, Daniel/0000-0001-7779-7765
NR 15
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U1 4
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 479
EP 501
DI 10.1007/s11214-012-9893-1
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500013
ER
PT J
AU Hassler, DM
Zeitlin, C
Wimmer-Schweingruber, RF
Bottcher, S
Martin, C
Andrews, J
Bohm, E
Brinza, DE
Bullock, MA
Burmeister, S
Ehresmann, B
Epperly, M
Grinspoon, D
Kohler, J
Kortmann, O
Neal, K
Peterson, J
Posner, A
Rafkin, S
Seimetz, L
Smith, KD
Tyler, Y
Weigle, G
Reitz, G
Cucinotta, FA
AF Hassler, D. M.
Zeitlin, C.
Wimmer-Schweingruber, R. F.
Boettcher, S.
Martin, C.
Andrews, J.
Boehm, E.
Brinza, D. E.
Bullock, M. A.
Burmeister, S.
Ehresmann, B.
Epperly, M.
Grinspoon, D.
Koehler, J.
Kortmann, O.
Neal, K.
Peterson, J.
Posner, A.
Rafkin, S.
Seimetz, L.
Smith, K. D.
Tyler, Y.
Weigle, G.
Reitz, G.
Cucinotta, F. A.
TI The Radiation Assessment Detector (RAD) Investigation
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE MSL; Mars Science Laboratory; Mars; Mars radiation environment;
Radiation; Human exploration detectors in space
ID GENERAL-CIRCULATION MODEL; GALACTIC COSMIC-RAYS; EARLY MARS; ORGANIC
SCINTILLATORS; MARTIAN ENVIRONMENT; ION PRODUCTION; SPACE; SURFACE;
ATMOSPHERE; DEPOSITS
AB The Radiation Assessment Detector (RAD) on the Mars Science Laboratory (MSL) is an energetic particle detector designed to measure a broad spectrum of energetic particle radiation. It will make the first-ever direct radiation measurements on the surface of Mars, detecting galactic cosmic rays, solar energetic particles, secondary neutrons, and other secondary particles created both in the atmosphere and in the Martian regolith. The radiation environment on Mars, both past and present, may have implications for habitability and the ability to sustain life. Radiation exposure is also a major concern for future human missions. The RAD instrument combines charged- and neutral-particle detection capability over a wide dynamic range in a compact, low-mass, low-power instrument. These capabilities are required in order to measure all the important components of the radiation environment.
RAD consists of the RAD Sensor Head (RSH) and the RAD Electronics Box (REB) integrated together in a small, compact volume. The RSH contains a solid-state detector telescope with three silicon PIN diodes for charged particle detection, a thallium doped Cesium Iodide scintillator, plastic scintillators for neutron detection and anti-coincidence shielding, and the front-end electronics. The REB contains three circuit boards, one with a novel mixed-signal ASIC for processing analog signals and an associated control FPGA, another with a second FPGA to communicate with the rover and perform onboard analysis of science data, and a third board with power supplies and power cycling or "sleep"-control electronics. The latter enables autonomous operation, independent of commands from the rover. RAD is a highly capable and highly configurable instrument that paves the way for future compact energetic particle detectors in space.
C1 [Hassler, D. M.; Zeitlin, C.; Andrews, J.; Bullock, M. A.; Ehresmann, B.; Neal, K.; Peterson, J.; Rafkin, S.] SW Res Inst, Boulder, CO USA.
[Wimmer-Schweingruber, R. F.; Boettcher, S.; Martin, C.; Boehm, E.; Burmeister, S.; Koehler, J.; Kortmann, O.; Seimetz, L.] Univ Kiel, Kiel, Germany.
[Brinza, D. E.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Epperly, M.; Smith, K. D.; Tyler, Y.; Weigle, G.] SW Res Inst, San Antonio, TX USA.
[Grinspoon, D.] Denver Museum Nat & Sci, Denver, CO USA.
[Kortmann, O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Posner, A.] NASA Headquarters, Washington, DC USA.
[Reitz, G.] Deutsch Zentrum Luft & Raumfahrt, Cologne, Germany.
[Cucinotta, F. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Hassler, DM (reprint author), SW Res Inst, Boulder, CO USA.
EM hassler@boulder.swri.edu
OI Posner, Arik/0000-0003-1572-8734
FU NASA (HEOMD) under JPL [1273039]; DLR; DLR's Space Administration
[50QM0501]
FX RAD is supported by NASA (HEOMD) under JPL subcontract #1273039 to
Southwest Research Institute and in Germany by DLR and DLR's Space
Administration grant 50QM0501 to the Christian-Albrechts-University
(CAU) Kiel. We would like to extend a huge thanks to Jeff Simmonds (MSL
Payload Manager) and the Project Science Team John Grotzinger, Joy
Crisp, and Ashwin Vasvada, the NASA Program Scientist Michael Meyer, and
the first Project Scientist Edward Stolper. We would also like to extend
a special thanks to Chris Moore and Gale Allen at NASA HQ (HEOMD) and
Heiner Witte at DLR in Germany for their unwavering support of RAD over
the years. Support for RAD calibration beam time at BNL/NSRL has been
provided by the NASA HRP Program. We also thank the management and
operators of the HIMAC facility at NIRS (Chiba, Japan), TSL in Uppsala,
Sweden, and iThemba Labs in South Africa for their many hours of
excellent beam time and support of RAD calibration.
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SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 503
EP 558
DI 10.1007/s11214-012-9913-1
PG 56
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500014
ER
PT J
AU Mitrofanov, IG
Litvak, ML
Varenikov, AB
Barmakov, YN
Behar, A
Bobrovnitsky, YI
Bogolubov, EP
Boynton, WV
Harshman, K
Kan, E
Kozyrev, AS
Kuzmin, RO
Malakhov, AV
Mokrousov, MI
Ponomareva, SN
Ryzhkov, VI
Sanin, AB
Smirnov, GA
Shvetsov, VN
Timoshenko, GN
Tomilina, TM
Tret'yakov, VI
Vostrukhin, AA
AF Mitrofanov, I. G.
Litvak, M. L.
Varenikov, A. B.
Barmakov, Y. N.
Behar, A.
Bobrovnitsky, Y. I.
Bogolubov, E. P.
Boynton, W. V.
Harshman, K.
Kan, E.
Kozyrev, A. S.
Kuzmin, R. O.
Malakhov, A. V.
Mokrousov, M. I.
Ponomareva, S. N.
Ryzhkov, V. I.
Sanin, A. B.
Smirnov, G. A.
Shvetsov, V. N.
Timoshenko, G. N.
Tomilina, T. M.
Tret'yakov, V. I.
Vostrukhin, A. A.
TI Dynamic Albedo of Neutrons (DAN) Experiment Onboard NASA's Mars Science
Laboratory
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars exploration; Detection of water; Active neutron experiment
ID LUNAR RECONNAISSANCE ORBITER; HEND INSTRUMENT ONBOARD; MESSENGER
GAMMA-RAY; ODYSSEY SPACECRAFT; SPECTROMETER DATA; EXPERIMENT LEND;
DETECTOR; SURFACE; HYDROGEN; WATER
AB The description of Dynamic Albedo of Neutrons (DAN) experiment is presented, as a part of the NASA's Mars Science Laboratory mission onboard the mars rover Curiosity. The instrument DAN includes Pulsing Neutron Generator (PNG) producing pulses of 14.1 MeV neutrons for irradiation of subsurface material below the rover, and Detectors and Electronics (DE) unit, which operates the instrument itself and measures the die-away time profiles of epithermal and thermal neutrons following each neutron pulse. It is shown that the DAN investigation will measure a content of hydrogen along the path of the MSL rover, and it will also provide information about a depth distribution of hydrogen at 10-20 regions selected for the detailed studies and sampling analysis.
C1 [Mitrofanov, I. G.; Litvak, M. L.; Varenikov, A. B.; Kozyrev, A. S.; Kuzmin, R. O.; Malakhov, A. V.; Mokrousov, M. I.; Sanin, A. B.; Tret'yakov, V. I.; Vostrukhin, A. A.] Space Res Inst, Moscow 117997, Russia.
[Barmakov, Y. N.; Bogolubov, E. P.; Ryzhkov, V. I.; Smirnov, G. A.] All Russian Inst Automat, Moscow 101000, Russia.
[Behar, A.; Kan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bobrovnitsky, Y. I.; Ponomareva, S. N.; Tomilina, T. M.] AA Blagonravov Mech Engn Inst, Moscow 101990, Russia.
[Boynton, W. V.; Harshman, K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Shvetsov, V. N.; Timoshenko, G. N.] Joint Inst Nucl Res, Dubna, Russia.
RP Mitrofanov, IG (reprint author), Space Res Inst, Profsouznaya St 84-32, Moscow 117997, Russia.
EM imitrofa@space.ru
FU International Space Science Institute (ISSI, Bern, Switzerland)
FX We wish to thank the International Space Science Institute (ISSI, Bern,
Switzerland) for the support of researches (included in the framework of
international team "Nuclear Planetology" in 2007-2010) presented in this
paper.
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EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 559
EP 582
DI 10.1007/s11214-012-9924-y
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500015
ER
PT J
AU Gomez-Elvira, J
Armiens, C
Castaner, L
Dominguez, M
Genzer, M
Gomez, F
Haberle, R
Harri, AM
Jimenez, V
Kahanpaa, H
Kowalski, L
Lepinette, A
Martin, J
Martinez-Frias, J
McEwan, I
Mora, L
Moreno, J
Navarro, S
de Pablo, MA
Peinado, V
Pena, A
Polkko, J
Ramos, M
Renno, NO
Ricart, J
Richardson, M
Rodriguez-Manfredi, J
Romeral, J
Sebastian, E
Serrano, J
Juarez, MD
Torres, J
Torrero, F
Urqui, R
Vazquez, L
Velasco, T
Verdasca, J
Zorzano, MP
Martin-Torres, J
AF Gomez-Elvira, J.
Armiens, C.
Castaner, L.
Dominguez, M.
Genzer, M.
Gomez, F.
Haberle, R.
Harri, A. -M.
Jimenez, V.
Kahanpaa, H.
Kowalski, L.
Lepinette, A.
Martin, J.
Martinez-Frias, J.
McEwan, I.
Mora, L.
Moreno, J.
Navarro, S.
de Pablo, M. A.
Peinado, V.
Pena, A.
Polkko, J.
Ramos, M.
Renno, N. O.
Ricart, J.
Richardson, M.
Rodriguez-Manfredi, J.
Romeral, J.
Sebastian, E.
Serrano, J.
Juarez, M. de la Torre
Torres, J.
Torrero, F.
Urqui, R.
Vazquez, L.
Velasco, T.
Verdasca, J.
Zorzano, M. -P.
Martin-Torres, J.
TI REMS: The Environmental Sensor Suite for the Mars Science Laboratory
Rover
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Mars Science Laboratory; Atmosphere; Meteorology; Pressure;
Relative Humidity; Wind; Ultraviolet radiation; Temperature
ID MARTIAN ATMOSPHERE; BOUNDARY-LAYER; ULTRAVIOLET SPECTROMETER; PRESSURE
PROFILE; LANDING SITE; DUST DEVILS; SURFACE; MODEL; INSTRUMENT;
PATHFINDER
AB The Rover Environmental Monitoring Station (REMS) will investigate environmental factors directly tied to current habitability at the Martian surface during the Mars Science Laboratory (MSL) mission. Three major habitability factors are addressed by REMS: the thermal environment, ultraviolet irradiation, and water cycling. The thermal environment is determined by a mixture of processes, chief amongst these being the meteorological. Accordingly, the REMS sensors have been designed to record air and ground temperatures, pressure, relative humidity, wind speed in the horizontal and vertical directions, as well as ultraviolet radiation in different bands. These sensors are distributed over the rover in four places: two booms located on the MSL Remote Sensing Mast, the ultraviolet sensor on the rover deck, and the pressure sensor inside the rover body. Typical daily REMS observations will collect 180 minutes of data from all sensors simultaneously (arranged in 5 minute hourly samples plus 60 additional minutes taken at times to be decided during the course of the mission). REMS will add significantly to the environmental record collected by prior missions through the range of simultaneous observations including water vapor; the ability to take measurements routinely through the night; the intended minimum of one Martian year of observations; and the first measurement of surface UV irradiation. In this paper, we describe the scientific potential of REMS measurements and describe in detail the sensors that constitute REMS and the calibration procedures.
C1 [Gomez-Elvira, J.; Armiens, C.; Gomez, F.; Lepinette, A.; Martin, J.; Martinez-Frias, J.; Mora, L.; Navarro, S.; Peinado, V.; Rodriguez-Manfredi, J.; Romeral, J.; Sebastian, E.; Torres, J.; Verdasca, J.; Zorzano, M. -P.; Martin-Torres, J.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain.
[McEwan, I.; Richardson, M.] Ashima Res, Pasadena, CA USA.
[Castaner, L.; Dominguez, M.; Jimenez, V.; Kowalski, L.; Ricart, J.] Univ Politecn Cataluna, E-08028 Barcelona, Spain.
[de Pablo, M. A.; Ramos, M.] Univ Alcala de Henares, Alcala De Henares, Spain.
[Juarez, M. de la Torre] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Moreno, J.; Pena, A.; Serrano, J.; Torrero, F.; Velasco, T.] EADS CRISA, Tres Cantos, Spain.
[Renno, N. O.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Genzer, M.; Harri, A. -M.; Kahanpaa, H.; Polkko, J.] FMI, Helsinki, Finland.
[Haberle, R.] NASA, Ames Res Ctr, Moffett Field, CA USA.
[Urqui, R.] INSA, Madrid, Spain.
[Vazquez, L.] Univ Complutence Madrid, Madrid, Spain.
RP Gomez-Elvira, J (reprint author), Ctr Astrobiol CSIC INTA, Carretera Ajalvir,Km 4, Madrid 28850, Spain.
EM gomezej@cab.inta-csic.es
RI Zorzano, Maria-Paz/F-2184-2015; Harri, Ari-Matti/C-7142-2012; de Pablo,
Miguel Angel/J-6442-2014; Gomez-Elvira, Javier/K-5829-2014; Ramos,
Miguel/K-2230-2014; JUAREZ, MANUELA/F-6674-2013; Urqui,
Roser/L-4862-2014; Gomez, Felipe/L-7315-2014; Rodriguez-Manfredi,
Jose/L-8001-2014; Zorzano, Maria-Paz/C-5784-2015; Martin-Torres,
Francisco Javier/G-6329-2015; Dominguez-Pumar, Manuel/K-9175-2015
OI Zorzano, Maria-Paz/0000-0002-4492-9650; Kahanpaa,
Henrik/0000-0001-9108-186X; Romeral Planello, Julio
Jose/0000-0002-2205-067X; Vazquez, Luis/0000-0003-4054-1197; Harri,
Ari-Matti/0000-0001-8541-2802; de Pablo, Miguel
Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846;
Ramos, Miguel/0000-0003-3648-6818; Urqui, Roser/0000-0001-6090-8502;
Gomez, Felipe/0000-0001-9977-7060; Rodriguez-Manfredi,
Jose/0000-0003-0461-9815; Zorzano, Maria-Paz/0000-0002-4492-9650;
Martin-Torres, Francisco Javier/0000-0001-6479-2236; Dominguez-Pumar,
Manuel/0000-0001-5439-7953
FU Centro de Desarrollo Tecnologico e Industrial (CDTI), Ministerio de
Economia y Competitividad [ESP2006-27267, ESP2007-65862, AYA2011-25720];
Instituto Nacional de Tecnica Aeroespacial (INTA) of Spain
FX The authors thanks to the Centro de Desarrollo Tecnologico e Industrial
(CDTI), Ministerio de Economia y Competitividad (ESP2006-27267,
ESP2007-65862, AYA2011-25720) and Instituto Nacional de Tecnica
Aeroespacial (INTA) of Spain for funding the project.
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SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 583
EP 640
DI 10.1007/s11214-012-9921-1
PG 58
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500016
ER
PT J
AU Golombek, M
Grant, J
Kipp, D
Vasavada, A
Kirk, R
Fergason, R
Bellutta, P
Calef, F
Larsen, K
Katayama, Y
Huertas, A
Beyer, R
Chen, A
Parker, T
Pollard, B
Lee, S
Sun, Y
Hoover, R
Sladek, H
Grotzinger, J
Welch, R
Dobrea, EN
Michalski, J
Watkins, M
AF Golombek, M.
Grant, J.
Kipp, D.
Vasavada, A.
Kirk, R.
Fergason, R.
Bellutta, P.
Calef, F.
Larsen, K.
Katayama, Y.
Huertas, A.
Beyer, R.
Chen, A.
Parker, T.
Pollard, B.
Lee, S.
Sun, Y.
Hoover, R.
Sladek, H.
Grotzinger, J.
Welch, R.
Dobrea, E. Noe
Michalski, J.
Watkins, M.
TI Selection of the Mars Science Laboratory Landing Site
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Landing sites; Mars; Surface materials; Surface characteristics; Mars
Science Laboratory
ID THERMAL EMISSION SPECTROMETER; ORBITER LASER ALTIMETER; SIZE-FREQUENCY
DISTRIBUTIONS; MAWRTH-VALLIS REGION; REMOTE-SENSING DATA; GALE-CRATER;
PHYSICAL-PROPERTIES; EXPLORATION ROVERS; MELAS-CHASMA; LAYERED DEPOSITS
AB The selection of Gale crater as the Mars Science Laboratory landing site took over five years, involved broad participation of the science community via five open workshops, and narrowed an initial > 50 sites (25 by 20 km) to four finalists (Eberswalde, Gale, Holden and Mawrth) based on science and safety. Engineering constraints important to the selection included: (1) latitude (+/- 30A degrees) for thermal management of the rover and instruments, (2) elevation (<-1 km) for sufficient atmosphere to slow the spacecraft, (3) relief of < 100-130 m at baselines of 1-1000 m for control authority and sufficient fuel during powered descent, (4) slopes of < 30A degrees at baselines of 2-5 m for rover stability at touchdown, (5) moderate rock abundance to avoid impacting the belly pan during touchdown, and (6) a radar-reflective, load-bearing, and trafficable surface that is safe for landing and roving and not dominated by fine-grained dust. Science criteria important for the selection include the ability to assess past habitable environments, which include diversity, context, and biosignature (including organics) preservation. Sites were evaluated in detail using targeted data from instruments on all active orbiters, and especially Mars Reconnaissance Orbiter. All of the final four sites have layered sedimentary rocks with spectral evidence for phyllosilicates that clearly address the science objectives of the mission. Sophisticated entry, descent and landing simulations that include detailed information on all of the engineering constraints indicate all of the final four sites are safe for landing. Evaluation of the traversabilty of the landing sites and target "go to" areas outside of the ellipse using slope and material properties information indicates that all are trafficable and "go to" sites can be accessed within the lifetime of the mission. In the final selection, Gale crater was favored over Eberswalde based on its greater diversity and potential habitability.
C1 [Golombek, M.; Kipp, D.; Vasavada, A.; Bellutta, P.; Calef, F.; Katayama, Y.; Huertas, A.; Chen, A.; Parker, T.; Pollard, B.; Lee, S.; Sun, Y.; Hoover, R.; Sladek, H.; Welch, R.; Dobrea, E. Noe; Michalski, J.; Watkins, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grant, J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
[Kirk, R.; Fergason, R.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Larsen, K.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Katayama, Y.] Japan Aerosp Explorat Agcy, Lunar & Planetary Explorat Program Grp, Tokyo, Japan.
[Beyer, R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sun, Y.; Grotzinger, J.] CALTECH, Pasadena, CA 91125 USA.
[Hoover, R.] Univ Colorado, Boulder, CO 80309 USA.
[Sladek, H.] Univ Montana Western, Dillon, MT 59725 USA.
[Dobrea, E. Noe; Michalski, J.] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Golombek, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mgolombek@jpl.nasa.gov
OI Beyer, Ross/0000-0003-4503-3335
FU Mars Data Analysis Program; Critical Data Products program
FX Research described in this paper was partially done by the MSL project,
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration and was
supported by the Mars Data Analysis Program. Derived data products were
sponsored by the Critical Data Products program administered by the JPL
Mars Exploration Program office. We especially thank members of the
Council of Atmospheres and Council of Terrains for work on
characterizing MSL landing sites. We thank L. Redmond and N. Warner for
help with the figures.
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SN 0038-6308
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J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 641
EP 737
DI 10.1007/s11214-012-9916-y
PG 97
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500017
ER
PT J
AU Fergason, RL
Christensen, PR
Golombek, MP
Parker, TJ
AF Fergason, R. L.
Christensen, P. R.
Golombek, M. P.
Parker, T. J.
TI Surface Properties of the Mars Science Laboratory Candidate Landing
Sites: Characterization from Orbit and Predictions
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Surface properties; Thermal inertia; MSL
ID THERMAL EMISSION SPECTROMETER; MAWRTH-VALLIS REGION; GALE-CRATER;
ATMOSPHERIC OBSERVATIONS; INTERANNUAL VARIABILITY; LASER ALTIMETER;
CLAY-MINERALS; PARTICLE-SIZE; HOLDEN CRATER; THEMIS DATA
AB This work describes the interpretation of THEMIS-derived thermal inertia data at the Eberswalde, Gale, Holden, and Mawrth Vallis Mars Science Laboratory (MSL) candidate landing sites and determines how thermophysical variations correspond to morphology and, when apparent, mineralogical diversity. At Eberswalde, the proportion of likely unconsolidated material relative to exposed bedrock or highly indurated surfaces controls the thermal inertia of a given region. At Gale, the majority of the landing site region has a moderate thermal inertia (250 to 410 J m(-2) K-1 s(-1/2)), which is likely an indurated surface mixed with unconsolidated materials. The primary difference between higher and moderate thermal inertia surfaces may be due to the amount of mantling material present. Within the mound of stratified material in Gale, layers are distinguished in the thermal inertia data; the MSL rover could be traversing through materials that are both thermophysically and compositionally diverse. The majority of the Holden ellipse has a thermal inertia of 340 to 475 J m(-2) K-1 s(-1/2) and consists of bed forms with some consolidated material intermixed. Mawrth Vallis has a mean thermal inertia of 310 J m(-2) K-1 s(-1/2) and a wide variety of materials is present contributing to the moderate thermal inertia surfaces, including a mixture of bedrock, indurated surfaces, bed forms, and unconsolidated fines. Phyllosilicates have been identified at all four candidate landing sites, and these clay-bearing units typically have a similar thermal inertia value (400 to 500 J m(-2) K-1 s(-1/2)), suggesting physical properties that are also similar.
C1 [Fergason, R. L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Christensen, P. R.] Arizona State Univ, Mars Space Flight Facil, Tempe, AZ 86287 USA.
[Golombek, M. P.; Parker, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fergason, RL (reprint author), US Geol Survey, Astrogeol Sci Ctr, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA.
EM rfergason@usgs.gov
FU Mars Odyssey Project Office; JPL
FX Attendance at the landing site workshops greatly enhanced our
understanding of various components of each site. Specifically,
discussions with Kenneth Edgett (MSSS), Justin Hagerty (USGS), Michael
Kraft (ASU), and Ashwin Vasavada (JPL) on various aspects related to
these sites greatly helped place our findings in a broader context.
Kenneth Herkenhoff (USGS), Kenneth Tanaka (USGS), Kenneth Edgett (MSSS),
and an anonymous reviewer provided comments that greatly improved the
presentation of this work. Trent Hare (USGS) and Ryan Luk (then at ASU)
helped produce products that have been released to the public
(http://astrogeology.usgs.gov/MSL/; http://themis.asu.edu/landingsites).
Ryan Luk was invaluable for helping develop mosaic scripts and
generating early versions of the daytime IR, nighttime IR, and visible
mosaics and the nighttime IR over daytime IR overlay images available
online. Daytime IR, nighttime IR, qualitative (8-bit) thermal inertia,
and visible image mosaic generation for the initial 36 proposed landing
sites (as of June 2006) was funded by the Mars Odyssey Project Office.
The thermal inertia analysis and generation and analysis of predicted
temperature maps were funded by a JPL subcontract through the Critical
Data Products program.
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SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 739
EP 773
DI 10.1007/s11214-012-9891-3
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500018
ER
PT J
AU Beyer, RA
Kirk, RL
AF Beyer, Ross A.
Kirk, Randolph L.
TI Meter-Scale Slopes of Candidate MSL Landing Sites from Point
Photoclinometry
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Mars Science Laboratory; Remote sensing
ID ORBITER LASER ALTIMETER; MARS; ROUGHNESS; CAMERA; PREDICTIONS; IMAGES;
LANDER
AB Photoclinometry was used to analyze the small-scale roughness of areas within the proposed Mars Science Laboratory (MSL) landing ellipses. The landing ellipses presented in this study are those in Eberswalde crater, Gale crater, and Holden crater (the Mawrth Vallis site could not be measured due to its albedo variations). We were able to constrain surface slopes on length scales comparable to the HiRISE image resolution (0.25 meters/pixel). The MSL mission has various engineering constraints that each candidate landing ellipse must satisfy. These constraints indicate that the statistical value of the slopes at one, two, and five meter baselines are an important criterion. We used our technique to estimate surface slopes across large swaths of each image, and built up slope statistics for the images in each landing ellipse. We are confident that all three final MSL landing site ellipses that could be measured in this study are within the small-scale roughness constraints. Our results have provided input into the landing hazard assessment process.
C1 [Beyer, Ross A.] SETI Inst, Carl Sagan Ctr, Moffett Field, CA USA.
[Beyer, Ross A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kirk, Randolph L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
RP Beyer, RA (reprint author), SETI Inst, Carl Sagan Ctr, Moffett Field, CA USA.
EM Ross.A.Beyer@nasa.gov
OI Beyer, Ross/0000-0003-4503-3335
FU National Aeronautics and Space Administration
FX We would like to thank the anonymous reviewers for insightful and
constructive reviews of this paper. This research has made use of NASA's
Astrophysics Data System and the USGS Integrated Software for Imagers
and Spectrometers (ISIS). This material is based upon work supported by
the National Aeronautics and Space Administration under awards issued
through the Mars Reconnaissance Orbiter program. We thank Fred Calef for
providing the HiRISE and CTX mosaic in the background of Figs. 8, 9, and
10.
NR 31
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U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 775
EP 791
DI 10.1007/s11214-012-9925-x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500019
ER
PT J
AU Vasavada, AR
Chen, A
Barnes, JR
Burkhart, PD
Cantor, BA
Dwyer-Cianciolo, AM
Fergason, RL
Hinson, DP
Justh, HL
Kass, DM
Lewis, SR
Mischna, MA
Murphy, JR
Rafkin, SCR
Tyler, D
Withers, PG
AF Vasavada, Ashwin R.
Chen, Allen
Barnes, Jeffrey R.
Burkhart, P. Daniel
Cantor, Bruce A.
Dwyer-Cianciolo, Alicia M.
Fergason, Robin L.
Hinson, David P.
Justh, Hilary L.
Kass, David M.
Lewis, Stephen R.
Mischna, Michael A.
Murphy, James R.
Rafkin, Scot C. R.
Tyler, Daniel
Withers, Paul G.
TI Assessment of Environments for Mars Science Laboratory Entry, Descent,
and Surface Operations
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Mars' atmosphere; Mars' surface; Spacecraft
ID THERMAL EMISSION SPECTROMETER; GENERAL-CIRCULATION MODEL; RADIO
OCCULTATION MEASUREMENTS; DELTA-EDDINGTON APPROXIMATION; CONVECTIVE
BOUNDARY-LAYER; ENCIRCLING DUST STORM; NORTH POLAR-REGION; GLOBAL
SURVEYOR; MARTIAN ATMOSPHERE; DATA ASSIMILATION
AB The Mars Science Laboratory mission aims to land a car-sized rover on Mars' surface and operate it for at least one Mars year in order to assess whether its field area was ever capable of supporting microbial life. Here we describe the approach used to identify, characterize, and assess environmental risks to the landing and rover surface operations. Novel entry, descent, and landing approaches will be used to accurately deliver the 900-kg rover, including the ability to sense and "fly out" deviations from a best-estimate atmospheric state. A joint engineering and science team developed methods to estimate the range of potential atmospheric states at the time of arrival and to quantitatively assess the spacecraft's performance and risk given its particular sensitivities to atmospheric conditions. Numerical models are used to calculate the atmospheric parameters, with observations used to define model cases, tune model parameters, and validate results. This joint program has resulted in a spacecraft capable of accessing, with minimal risk, the four finalist sites chosen for their scientific merit. The capability to operate the landed rover over the latitude range of candidate landing sites, and for all seasons, was verified against an analysis of surface environmental conditions described here. These results, from orbital and model data sets, also drive engineering simulations of the rover's thermal state that are used to plan surface operations.
C1 [Vasavada, Ashwin R.; Chen, Allen; Burkhart, P. Daniel; Kass, David M.; Mischna, Michael A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Barnes, Jeffrey R.; Tyler, Daniel] Oregon State Univ, Corvallis, OR 97331 USA.
[Cantor, Bruce A.] Malin Space Sci Syst, San Diego, CA USA.
[Dwyer-Cianciolo, Alicia M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Fergason, Robin L.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Hinson, David P.] SETI Inst, Mountain View, CA USA.
[Justh, Hilary L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Lewis, Stephen R.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Murphy, James R.] New Mexico State Univ, Las Cruces, NM 88003 USA.
[Rafkin, Scot C. R.] SW Res Inst, Boulder, CO USA.
[Withers, Paul G.] Boston Univ, Boston, MA 02215 USA.
RP Vasavada, AR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ashwin@jpl.nasa.gov
RI Withers, Paul/H-2241-2014;
OI Lewis, Stephen/0000-0001-7237-6494
NR 85
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U1 0
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 793
EP 835
DI 10.1007/s11214-012-9911-3
PG 43
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500020
ER
PT J
AU Hu, CM
Feng, L
Lee, Z
Davis, CO
Mannino, A
McClain, CR
Franz, BA
AF Hu, Chuanmin
Feng, Lian
Lee, Zhongping
Davis, Curtiss O.
Mannino, Antonio
McClain, Charles R.
Franz, Bryan A.
TI Dynamic range and sensitivity requirements of satellite ocean color
sensors: learning from the past
SO APPLIED OPTICS
LA English
DT Article
ID SIGNAL-TO-NOISE; CHLOROPHYLL FLUORESCENCE; ATMOSPHERIC CORRECTION;
COASTAL WATERS; EO-1 HYPERION; ALGORITHM; PHYTOPLANKTON; MODEL; MODIS;
OPTIMIZATION
AB Sensor design and mission planning for satellite ocean color measurements requires careful consideration of the signal dynamic range and sensitivity (specifically here signal-to-noise ratio or SNR) so that small changes of ocean properties (e.g., surface chlorophyll-a concentrations or Chl) can be quantified while most measurements are not saturated. Past and current sensors used different signal levels, formats, and conventions to specify these critical parameters, making it difficult to make cross-sensor comparisons or to establish standards for future sensor design. The goal of this study is to quantify these parameters under uniform conditions for widely used past and current sensors in order to provide a reference for the design of future ocean color radiometers. Using measurements from the Moderate Resolution Imaging Spectroradiometer onboard the Aqua satellite (MODISA) under various solar zenith angles (SZAs), typical (L-typical) and maximum (L-max) at-sensor radiances from the visible to the shortwave IR were determined. The L-typical values at an SZA of 45 degrees were used as constraints to calculate SNRs of 10 multiband sensors at the same L-typical radiance input and 2 hyperspectral sensors at a similar radiance input. The calculations were based on clear-water scenes with an objective method of selecting pixels with minimal cross-pixel variations to assure target homogeneity. Among the widely used ocean color sensors that have routine global coverage, MODISA ocean bands (1 km) showed 2-4 times higher SNRs than the Sea-viewing Wide Field-of-view Sensor (Sea-WiFS) (1 km) and comparable SNRs to the Medium Resolution Imaging Spectrometer (MERIS)-RR (reduced resolution, 1.2 km), leading to different levels of precision in the retrieved Chl data product. MERIS-FR (full resolution, 300 m) showed SNRs lower than MODISA and MERIS-RR with the gain in spatial resolution. SNRs of all MODISA ocean bands and SeaWiFS bands (except the SeaWiFS near-IR bands) exceeded those from prelaunch sensor specifications after adjusting the input radiance to L-typical. The tabulated L-typical, L-max, and SNRs of the various multiband and hyperspectral sensors under the same or similar radiance input provide references to compare sensor performance in product precision and to help design future missions such as the Geostationary Coastal and Air Pollution Events (GEO-CAPE) mission and the Pre-Aerosol-Clouds-Ecosystems (PACE) mission currently being planned by the U.S. National Aeronautics and Space Administration (NASA). (c) 2012 Optical Society of America
C1 [Hu, Chuanmin; Feng, Lian] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
[Feng, Lian] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430079, Peoples R China.
[Lee, Zhongping] Univ Massachusetts, Dept Environm Earth & Ocean Sci, Boston, MA 02125 USA.
[Davis, Curtiss O.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Mannino, Antonio; McClain, Charles R.; Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hu, CM (reprint author), Univ S Florida, Coll Marine Sci, 140 7th Ave S, St Petersburg, FL 33701 USA.
EM hu@marine.usf.edu
RI hu, chuanmin/J-5021-2012; Franz, Bryan/D-6284-2012; Mannino,
Antonio/I-3633-2014
OI Franz, Bryan/0000-0003-0293-2082;
FU state of Florida; U.S. NASA Ocean Biology and Biogeochemistry (OBB)
program; Water and Energy Cycle program
FX This work was supported by the state of Florida, the U.S. NASA Ocean
Biology and Biogeochemistry (OBB) program and the Water and Energy Cycle
program and inspired by numerous discussions within the GEO-CAPE science
definition team. Support of L. Feng has been provided by an education
program for visiting and exchanging students. We thank the various
agencies that provided satellite data in this study, including the NASA
Goddard Space Flight Center, U.S. Geological Survey, the European Space
Agency, the Earth Scan Lab of Louisiana University, Oregon State
University, and Korea Ocean Research and Development Institute (KORDI).
The authors thank Drs. M. Behrenfeld and T. Westberry (Oregon State
University) for their helpful discussions on MODIS FLH data products.
The manuscript benefited from substantial comments and suggestions
provided by three anonymous reviewers, whose contribution is
acknowledged.
NR 41
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U1 1
U2 32
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD SEP 1
PY 2012
VL 51
IS 25
BP 6045
EP 6062
DI 10.1364/AO.51.006045
PG 18
WC Optics
SC Optics
GA 003GF
UT WOS:000308595500015
PM 22945151
ER
PT J
AU Horst, SM
Yelle, RV
Buch, A
Carrasco, N
Cernogora, G
Dutuit, O
Quirico, E
Sciamma-O'Brien, E
Smith, MA
Somogyi, A
Szopa, C
Thissen, R
Vuitton, V
AF Hoerst, S. M.
Yelle, R. V.
Buch, A.
Carrasco, N.
Cernogora, G.
Dutuit, O.
Quirico, E.
Sciamma-O'Brien, E.
Smith, M. A.
Somogyi, A.
Szopa, C.
Thissen, R.
Vuitton, V.
TI Formation of Amino Acids and Nucleotide Bases in a Titan Atmosphere
Simulation Experiment
SO ASTROBIOLOGY
LA English
DT Article
DE Astrochemistry; Planetary atmospheres; Titan; Astrobiology
ID COUPLING PHOTOCHEMISTRY; ORGANIC-COMPOUND; PRIMITIVE EARTH; HAZE
FORMATION; GAS; THOLINS; CHEMISTRY; PLASMA; SPECTROMETER; MOLECULES
AB The discovery of large (> 100 u) molecules in Titan's upper atmosphere has heightened astrobiological interest in this unique satellite. In particular, complex organic aerosols produced in atmospheres containing C, N, O, and H, like that of Titan, could be a source of prebiotic molecules. In this work, aerosols produced in a Titan atmosphere simulation experiment with enhanced CO (N-2/CH4/CO gas mixtures of 96.2%/2.0%/1.8% and 93.2%/5.0%/1.8%) were found to contain 18 molecules with molecular formulae that correspond to biological amino acids and nucleotide bases. Very high-resolution mass spectrometry of isotopically labeled samples confirmed that C4H5N3O, C4H4N2O2, C5H6N2O2, C5H5N5, and C6H9N3O2 are produced by chemistry in the simulation chamber. Gas chromatography-mass spectrometry (GC-MS) analyses of the non-isotopic samples confirmed the presence of cytosine (C4H5N3O), uracil (C5H4N2O2), thymine (C5H6N2O2), guanine (C5H5N5O), glycine (C2H5NO2), and alanine (C3H7NO2). Adenine (C5H5N5) was detected by GC-MS in isotopically labeled samples. The remaining prebiotic molecules were detected in unlabeled samples only and may have been affected by contamination in the chamber. These results demonstrate that prebiotic molecules can be formed by the high-energy chemistry similar to that which occurs in planetary upper atmospheres and therefore identifies a new source of prebiotic material, potentially increasing the range of planets where life could begin.
C1 [Hoerst, S. M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Hoerst, S. M.; Yelle, R. V.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Buch, A.] Ecole Cent Paris, Lab Genie Proc & Mat, Paris, France.
[Carrasco, N.; Cernogora, G.; Szopa, C.] Univ Paris 06, Univ Versailles St Quentin, CNRS, UMPC,Lab Atm, Guyancourt, France.
[Dutuit, O.; Quirico, E.; Thissen, R.; Vuitton, V.] Univ Grenoble 1, CNRS, UMR 5109, Inst Planetol & Astrophys Grenoble, Grenoble, France.
[Sciamma-O'Brien, E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Smith, M. A.] Univ Houston, Coll Nat Sci & Math, Houston, TX USA.
[Smith, M. A.; Somogyi, A.] Univ Arizona, Dept Chem & Biochem, Tucson, AZ USA.
RP Horst, SM (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Box 216 UCB, Boulder, CO 80309 USA.
EM sarah.horst@colorado.edu
RI Horst, Sarah/A-9906-2010; quirico, eric/K-9650-2013; Carrasco,
Nathalie/D-2365-2012; Sciamma-O'Brien, Ella/M-2043-2014; szopa,
cyril/C-6865-2015
OI Horst, Sarah/0000-0003-4596-0702; quirico, eric/0000-0003-2768-0694;
Carrasco, Nathalie/0000-0002-0596-6336; Sciamma-O'Brien,
Ella/0000-0002-1883-552X; szopa, cyril/0000-0002-0090-4056
FU NSF Astronomy; Astrophysics Postdoctoral Fellowship [AST-1102827]; NASA
Earth and Space Sciences Fellowship [NNX08AX62H]; NASA Planetary
Atmospheres Grant [NNX09AB586]; JPL under the NASA Astrobiology
Institute [1372177]; NASA Exobiology Grant [NNG05GO58G]; Centre National
d'Etudes Spatiales (CNES), France; PRES UniverSud; CNES; Rhone-Alpes
region [ANR-07-BLAN-0123]; CNRS interdisciplinary program Origine des
Planetes de la Vie (OPV); ATIPE grant; European Commission for the Marie
Curie International Reintegration [231013]
FX S.M.H. is supported by NSF Astronomy and Astrophysics Postdoctoral
Fellowship AST-1102827. S.M.H. was also supported by NASA Earth and
Space Sciences Fellowship NNX08AX62H. S.M.H. and R.V.Y. are supported by
a NASA Planetary Atmospheres Grant NNX09AB586. S.M.H., R.V.Y., and
M.A.S. are supported by JPL subcontract 1372177 under the NASA
Astrobiology Institute. M.A.S. is supported by NASA Exobiology Grant
NNG05GO58G. E.Q. and R.T. acknowledge funding from the Centre National
d'Etudes Spatiales (CNES), France. E.S.O. was supported by postdoctoral
fellowships from PRES UniverSud and CNES. This work was partly supported
by ANR-07-BLAN-0123, Cible 2007 of the Rhone-Alpes region, the CNRS
interdisciplinary program Origine des Planetes de la Vie (OPV), and
CNES. R.T. thanks the CNRS Chemistry Institute for an ATIPE grant. V.V.
is grateful to the European Commission for the Marie Curie International
Reintegration Grant No. 231013.
NR 35
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U1 8
U2 109
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP
PY 2012
VL 12
IS 9
BP 809
EP 817
DI 10.1089/ast.2011.0623
PG 9
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 009WD
UT WOS:000309055200001
PM 22917035
ER
PT J
AU Mattioda, A
Cook, A
Ehrenfreund, P
Quinn, R
Ricco, AJ
Squires, D
Bramall, N
Bryson, K
Chittenden, J
Minelli, G
Agasid, E
Allamandola, L
Beasley, C
Burton, R
Defouw, G
Diaz-Aguado, M
Fonda, M
Friedericks, C
Kitts, C
Landis, D
Mclntyre, M
Neumann, M
Rasay, M
Ricks, R
Salama, F
Santos, O
Schooley, A
Yost, B
Young, A
AF Mattioda, Andrew
Cook, Amanda
Ehrenfreund, Pascale
Quinn, Richard
Ricco, Antonio J.
Squires, David
Bramall, Nathan
Bryson, Kathryn
Chittenden, Julie
Minelli, Giovanni
Agasid, Elwood
Allamandola, Lou
Beasley, Chris
Burton, Roland
Defouw, Greg
Diaz-Aguado, Millan
Fonda, Mark
Friedericks, Charles
Kitts, Chris
Landis, David
Mclntyre, Mike
Neumann, Michael
Rasay, Mike
Ricks, Robert
Salama, Farid
Santos, Orlando
Schooley, Aaron
Yost, Bruce
Young, Anthony
TI The O/OREOS Mission: First Science Data from the Space Environment
Viability of Organics (SEVO) Payload
SO ASTROBIOLOGY
LA English
DT Article
DE Cubesat; Nanosatellite; O/OREOS; SEVO; Low-Earth orbit; Astrobiology;
UV-visible spectroscopy; Photochemistry; Photodegradation of organics;
Polycyclic aromatic hydrocarbons; Quinone
ID POLYCYCLIC AROMATIC-HYDROCARBONS; NEAR-INFRARED SPECTROSCOPY;
ELECTRONIC-TRANSITIONS; ULTRAVIOLET PHOTOLYSIS; ICE ANALOGS; WATER;
METEORITES; MOLECULES; QUINONES; EXPOSURE
AB We report the first science results from the Space Environment Viability of Organics (SEVO) payload aboard the Organism/Organic Exposure to Orbital Stresses (O/OREOS) free-flying nanosatellite, which completed its nominal spaceflight mission in May 2011 but continues to acquire data biweekly. The SEVO payload integrates a compact UV-visible-NIR spectrometer, utilizing the Sun as its light source, with a 24-cell sample carousel that houses four classes of vacuum-deposited organic thin films: polycyclic aromatic hydrocarbon (PAH), amino acid, metalloporphyrin, and quinone. The organic films are enclosed in hermetically sealed sample cells that contain one of four astrobiologically relevant microenvironments. Results are reported in this paper for the first 309 days of the mission, during which the samples were exposed for similar to 2210 h to direct solar illumination (similar to 1080 kJ/cm(2) of solar energy over the 124-2600nm range). Transmission spectra (200-1000 nm) were recorded for each film, at first daily and subsequently every 15 days, along with a solar spectrum and the dark response of the detector array. Results presented here include eight preflight and 16 in-flight spectra of eight SEVO sample cells. Spectra from the PAH thin film in a water-vapor-containing microenvironment indicate measurable change due to solar irradiation in orbit, while three other nominally water-free microenvironments show no appreciable change. The quinone anthrarufin showed high photostability and no significant spectroscopically measurable change in any of the four microenvironments during the same period. The SEVO experiment provides the first in situ real-time analysis of the photostability of organic compounds and biomarkers in orbit.
C1 [Mattioda, Andrew; Cook, Amanda; Ricco, Antonio J.; Squires, David; Chittenden, Julie; Minelli, Giovanni; Agasid, Elwood; Allamandola, Lou; Beasley, Chris; Burton, Roland; Defouw, Greg; Diaz-Aguado, Millan; Fonda, Mark; Friedericks, Charles; Mclntyre, Mike; Ricks, Robert; Salama, Farid; Santos, Orlando; Schooley, Aaron; Yost, Bruce] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA.
[Quinn, Richard; Bramall, Nathan] SETI Inst, Mountain View, CA USA.
[Bryson, Kathryn] Bay Area Environm Res Inst, Sonoma, CA USA.
[Kitts, Chris; Neumann, Michael; Rasay, Mike; Young, Anthony] Santa Clara Univ, Robot Syst Lab, Santa Clara, CA USA.
[Landis, David] Charles Stark Draper Lab, Cambridge, MA USA.
RP Mattioda, A (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
EM andrew.mattioda@nasa.gov
RI Bryson, Kathryn/I-6914-2012; Salama, Farid/A-8787-2009;
OI Salama, Farid/0000-0002-6064-4401; Ricco, Antonio/0000-0002-2355-4984
FU NASA Astrobiology Small Payloads program; NASA; Exobiology Program
[09-EXOB09-1030]
FX The authors would like to thank the NASA Astrobiology Small Payloads
program for support, Robert Walker for outstanding technical support,
Emmett Quigley and Ryan Walker of the NASA Ames Airborne Instrument
Development Lab for their work in producing the hardware necessary for
the production of the sample cells, the NASA Astrobiology Institute, the
NASA Postdoctoral Program (NPP) administered by Oak Ridge Associated
Universities through a contract with NASA, and the Exobiology Program
for additional support (proposal number 09-EXOB09-1030). We also thank
Cindy Taylor for assistance with deposition and characterization of the
thin films, and members of the NASA Ames Small Spacecraft Payloads and
Technologies Team, including Michael Henschke, Lynn Hofland, Ed Luzzi,
Nghia Mai, Andrea Nazzal, and John Tucker. We are also grateful for the
efforts of the highly effective student- and-staff operations team at
Santa Clara University, including Laura Bica and Ignacio Mas. We
acknowledge helpful discussions and guidance from Andrew Holmes-Siedle
(REM Oxford, Ltd.), developer of the radFETs.
NR 39
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U2 24
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP
PY 2012
VL 12
IS 9
BP 841
EP 853
DI 10.1089/ast.2012.0861
PG 13
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 009WD
UT WOS:000309055200004
PM 22984872
ER
PT J
AU Mccoy, KB
Derecho, I
Wong, T
Tran, HM
Huynh, TD
La Duc, MT
Venkateswaran, K
Mogul, R
AF McCoy, K. B.
Derecho, I.
Wong, T.
Tran, H. M.
Huynh, T. D.
La Duc, M. T.
Venkateswaran, K.
Mogul, R.
TI Insights into the Extremotolerance of Acinetobacter radioresistens 50v1,
a Gram-Negative Bacterium Isolated from the Mars Odyssey Spacecraft
SO ASTROBIOLOGY
LA English
DT Article
DE Planetary protection; Spacecraft assembly facility; Extremophiles; Mars;
Microbe
ID FACULTATIVELY PSYCHROPHILIC BACTERIUM; HIGH CATALASE ACTIVITY;
HYDROGEN-PEROXIDE; ASSEMBLY FACILITY; PHOSPHATE RELEASE;
BACILLUS-PUMILUS; CLEAN ROOM; RESISTANCE; CALCOACETICUS; ENVIRONMENTS
AB The microbiology of the spacecraft assembly process is of paramount importance to planetary exploration, as the biological contamination that can result from remote-enabled spacecraft carries the potential to impact both life-detection experiments and extraterrestrial evolution. Accordingly, insights into the mechanisms and range of extremotolerance of Acinetobacter radioresistens 50v1, a Gram-negative bacterium isolated from the surface of the preflight Mars Odyssey orbiter, were gained by using a combination of microbiological, enzymatic, and proteomic methods. In summary, A. radioresistens 50v1 displayed a remarkable range of survival against hydrogen peroxide and the sequential exposures of desiccation, vapor and plasma phase hydrogen peroxide, and ultraviolet irradiation. The survival is among the highest reported for non-spore-forming and Gram-negative bacteria and is based upon contributions from the enzyme-based degradation of H2O2 (catalase and alkyl hydroperoxide reductase), energy management (ATP synthase and alcohol dehydrogenase), and modulation of the membrane composition. Together, the biochemical and survival features of A. radioresistens 50v1 support a potential persistence on Mars (given an unintended or planned surface landing of the Mars Odyssey orbiter), which in turn may compromise the scientific integrity of future life-detection missions.
C1 [Mogul, R.] Calif State Polytech Univ Pomona, Dept Chem, Pomona, CA 91768 USA.
[La Duc, M. T.; Venkateswaran, K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Mogul, R (reprint author), Calif State Polytech Univ Pomona, Dept Chem, 3801 W Temple Ave, Pomona, CA 91768 USA.
EM rmogul@csupomona.edu
FU NASA Astrobiology Institute Minority Institutional Research Support
program; NASA ROSES
FX These studies were supported by the NASA Astrobiology Institute Minority
Institutional Research Support program (R. Mogul) and in part by a NASA
ROSES 2003 award (K. Venkateswaran). The authors extend their gratitude
to Freida Dallal and Charlie Seto for biochemical support, Claire
Waggoner (IIRMES) for the proteomics work and discussions, and to the
Cal Poly Pomona new investigator funds and Science Educational
Enhancement Services program (SEES) for initial support.
NR 42
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U1 0
U2 22
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP
PY 2012
VL 12
IS 9
BP 854
EP 862
DI 10.1089/ast.2012.0835
PG 9
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 009WD
UT WOS:000309055200005
PM 22917036
ER
PT J
AU Mora, MF
Stockton, AM
Willis, PA
AF Mora, Maria F.
Stockton, Amanda M.
Willis, Peter A.
TI Microchip capillary electrophoresis instrumentation for in situ analysis
in the search for extraterrestrial life
SO ELECTROPHORESIS
LA English
DT Review
DE Extraterrestrial exploration; Laser-induced fluorescence; Microchip
capillary electrophoresis; Pneumatically actuated valves
ID MARS ORGANIC ANALYZER; TOTAL ANALYSIS SYSTEMS; MARTIAN METEORITE
ALH84001; NEUTRAL MASS-SPECTROMETER; INTERNAL STRUCTURE; MICROFLUIDIC
SYSTEMS; SUBSURFACE OCEAN; GENETIC-ANALYSIS; MEMBRANE VALVES;
AMINO-ACIDS
AB The search for signs of life on extraterrestrial planetary bodies is among NASA's top priorities in Solar System exploration. The associated pursuit of organics and biomolecules as evidence of past or present life demands in situ investigations of planetary bodies for which sample return missions are neither practical nor affordable. These in situ studies require instrumentation capable of sensitive chemical analyses of complex mixtures including a broad range of organic molecules. Instrumentation must also be capable of autonomous operation aboard a robotically controlled vehicle that collects data and transmits it back to Earth. Microchip capillary electrophoresis (mu CE) coupled to laser-induced fluorescence (LIF) detection provides this required sensitivity and targets a wide range of relevant organics while offering low mass, volume, and power requirements. Thus, this technology would be ideally suited for in situ studies of astrobiology targets, such as Mars, Europa, Enceladus, and Titan. In this review, we introduce the characteristics of these planetary bodies that make them compelling destinations for extraterrestrial astrobiological studies, and the principal groups of organics of interest associated with each. And although the technology we describe here was first developed specifically for proposed studies of Mars, by summarizing its evolution over the past decade, we demonstrate how mu CE-LIF instrumentation has become an ideal candidate for missions of exploration to all of these nearby worlds in our Solar System.
C1 [Mora, Maria F.; Stockton, Amanda M.; Willis, Peter A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Willis, PA (reprint author), Mail Stop 302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM peter.a.willis@jpl.nasa.gov
RI Mora, Maria/C-9753-2009; Willis, Peter/I-6621-2012
FU NASA's ASTID Program [104320]; NASA Postdoctoral Program (NPP) at the
Jet Propulsion Laboratory
FX The writing of this review was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Financial support was
provided by NASA's ASTID Program (Project #104320) and the NASA
Postdoctoral Program (NPP) at the Jet Propulsion Laboratory,
administered by Oak Ridge Associated Universities through a contract
with NASA.
NR 130
TC 19
Z9 19
U1 6
U2 76
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0173-0835
EI 1522-2683
J9 ELECTROPHORESIS
JI Electrophoresis
PD SEP
PY 2012
VL 33
IS 17
SI SI
BP 2624
EP 2638
DI 10.1002/elps.201200102
PG 15
WC Biochemical Research Methods; Chemistry, Analytical
SC Biochemistry & Molecular Biology; Chemistry
GA 003AS
UT WOS:000308581100003
PM 22965706
ER
PT J
AU Spatz, JM
Fields, EE
Yu, EW
Pajevic, PD
Bouxsein, ML
Sibonga, JD
Zwart, SR
Smith, SM
AF Spatz, J. M.
Fields, E. E.
Yu, E. W.
Pajevic, P. Divieti
Bouxsein, M. L.
Sibonga, J. D.
Zwart, S. R.
Smith, S. M.
TI Serum Sclerostin Increases in Healthy Adult Men during Bed Rest
SO JOURNAL OF CLINICAL ENDOCRINOLOGY & METABOLISM
LA English
DT Article
ID NUTRITIONAL-STATUS; BONE-FORMATION; EXPRESSION; SOST
AB Context: Animal models and human studies suggest that osteocytes regulate the skeleton's response to mechanical unloading in part by an increase in sclerostin. However, few studies have reported changes in serum sclerostin in humans exposed to reduced mechanical loading.
Objective: We determined changes in serum sclerostin and bone turnover markers in healthy adult men undergoing controlled bed rest.
Design, Setting, and Participants: Seven healthy adult men (31 +/- 3 yr old) underwent 90 d of 6 head down tilt bed rest at the University of Texas Medical Branch Institute for Translational Sciences-Clinical Research Center.
Outcomes: Serum sclerostin, PTH, vitamin D, bone resorption and formation markers, urinary calcium and phosphorus excretion, and 24-h pooled urinary markers of bone resorption were evaluated before bed rest [baseline (BL)] and at bed rest d 28 (BR-28), d 60 (BR-60), and d 90 (BR-90). Bone mineral density was measured at BL, BR-60, and 5 d after the end of the study (BR+5). Data are reported as mean +/- SD.
Results: Consistent with prior reports, bone mineral density declined significantly (1-2% per month) at weight-bearing skeletal sites. Serum sclerostin was elevated above BL at BR-28 (+29 +/- 20%; P = 0.003) and BR-60 (+42 +/- 31%; P < 0.001), with a lesser increase at BR-90 (+22 +/- 21%; P = 0.07). Serum PTH levels were reduced at BR-28 (-17 +/- 16%; P = 0.02) and BR-60 (-24 +/- 14%; P = 0.03) and remained lower than BL at BR-90 (-21 +/- 21%; P = 0.14), but did not reach statistical significance. Serum bone turnover markers were unchanged; however, urinary bone resorption markers and calcium were significantly elevated at all time points after bed rest (P < 0.01).
Conclusions: In healthy men subjected to controlled bed rest for 90 d, serum sclerostin increased, with a peak at 60, whereas serum PTH declined, and urinary calcium and bone resorption markers increased. (J Clin Endocrinol Metab 97: E1736-E1740, 2012)
C1 [Spatz, J. M.; Bouxsein, M. L.] Beth Israel Deaconess Med Ctr, Ctr Adv Orthoped Studies, Boston, MA 02215 USA.
[Spatz, J. M.; Bouxsein, M. L.] Harvard Univ, Sch Med, Boston, MA 02215 USA.
[Spatz, J. M.] Harvard Massachusetts Inst Technol, Div Hlth Sci & Technol, Cambridge, MA 02139 USA.
[Sibonga, J. D.; Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA.
[Spatz, J. M.; Yu, E. W.; Pajevic, P. Divieti; Bouxsein, M. L.] Massachusetts Gen Hosp, Endocrine Unit, Boston, MA 02114 USA.
[Fields, E. E.] Enterprise Advisory Serv Inc, Houston, TX 77058 USA.
[Zwart, S. R.] Univ Space Res Assoc, Houston, TX 77058 USA.
RP Spatz, JM (reprint author), Beth Israel Deaconess Med Ctr, Ctr Adv Orthoped Studies, RN 118,330 Brookline Ave, Boston, MA 02215 USA.
EM jspatz@bidmc.harvard.edu
FU NASA's Human Research Program [NASA NNX10AE39G]; National Institutes of
Health [R21 AR057522, UH2AR059655]; Harvard-Massachusetts Institute of
Technology Division of Health Sciences and Technology Bioastronautics
Ph.D. Program; Northrop Grumman Aerospace Systems Ph.D. Training
Fellowship
FX The authors acknowledge NASA's Human Research Program (NASA NNX10AE39G),
the National Institutes of Health (R21 AR057522, UH2AR059655),
Harvard-Massachusetts Institute of Technology Division of Health
Sciences and Technology Bioastronautics Ph.D. Program, and Northrop
Grumman Aerospace Systems Ph.D. Training Fellowship for providing
support for this work.
NR 19
TC 43
Z9 43
U1 0
U2 4
PU ENDOCRINE SOC
PI CHEVY CHASE
PA 8401 CONNECTICUT AVE, SUITE 900, CHEVY CHASE, MD 20815-5817 USA
SN 0021-972X
J9 J CLIN ENDOCR METAB
JI J. Clin. Endocrinol. Metab.
PD SEP
PY 2012
VL 97
IS 9
BP E1736
EP E1740
DI 10.1210/jc.2012-1579
PG 5
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA 004PF
UT WOS:000308692900014
PM 22767636
ER
PT J
AU Plante, I
Tippayamontri, T
Autsavapromporn, N
Meesungnoen, J
Jay-Gerin, JP
AF Plante, Ianik
Tippayamontri, Thititip
Autsavapromporn, Narongchai
Meesungnoen, Jintana
Jay-Gerin, Jean-Paul
TI Monte Carlo simulation of the radiolysis of the ceric sulfate dosimeter
by low linear energy transfer radiation
SO CANADIAN JOURNAL OF CHEMISTRY-REVUE CANADIENNE DE CHIMIE
LA English
DT Article
DE ceric sulfate dosimeter; radiolysis; free-radical and molecular yields;
linear energy transfer (LET); Monte Carlo simulations
ID SULFURIC-ACID-SOLUTIONS; LIQUID WATER; MOLECULAR YIELDS;
AQUEOUS-SOLUTIONS; IONIC-STRENGTH; PROTON TRACKS; FAST-ELECTRON;
RADICALS
AB The ceric sulfate dosimeter is based on the radio-induced reduction of Ce4+ in acidic medium. For low linear energy transfer (LET) radiation, the yield of Ce3+ is 2.4 molecules / 100 eV, regardless of the presence of oxygen. To investigate the reaction mechanisms of the ceric sulfate dosimeter, we simulated the chemical reaction kinetics curves and the evolution of G(Ce3+), G(O-2), and G(H-2) in the ceric sulfate solution with and without oxygen. Studies of G(Ce3+) as function of the initial concentration of Ce3+ and of the LET were also done. One important finding of this study is that (OH)-O-center dot radicals are scavenged by the reaction (OH)-O-center dot + HSO4- -> SO4 center dot- + H2O, rather than by the reaction (OH)-O-center dot + Ce3+ -> Ce4+ + OH-.
C1 [Plante, Ianik] Univ Space Res Assoc, NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Plante, Ianik; Tippayamontri, Thititip; Autsavapromporn, Narongchai; Meesungnoen, Jintana; Jay-Gerin, Jean-Paul] Univ Sherbrooke, Fac Med & Sci Sante, Dept Med Nucl & Radiobiol, Sherbrooke, PQ J1H 5N4, Canada.
[Autsavapromporn, Narongchai] Natl Inst Radiol Sci, Int Open Lab, Inage Ku, Chiba 2638555, Japan.
RP Plante, I (reprint author), Univ Space Res Assoc, NASA Johnson Space Ctr, 2101 NASA Pkwy,Bldg 37,Mail Code SK, Houston, TX 77058 USA.
EM Ianik.Plante-1@nasa.gov
OI autsavapromporn, narongchai/0000-0002-0189-3096
FU Natural Sciences and Engineering Research Council (NSERC) of Canada;
Canadian Space Agency; NSERC
FX The PhD studies of I. P. were supported by scholarships from the Natural
Sciences and Engineering Research Council (NSERC) of Canada and the
Canadian Space Agency. I. P. would also like to thank Dr. Francis A.
Cucinotta (NASA) for useful discussions. The financial assistance
provided by NSERC to J.-P.J.-G. is gratefully acknowledged.
NR 29
TC 3
Z9 3
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 0008-4042
J9 CAN J CHEM
JI Can. J. Chem.-Rev. Can. Chim.
PD SEP
PY 2012
VL 90
IS 9
BP 717
EP 723
DI 10.1139/V2012-052
PG 7
WC Chemistry, Multidisciplinary
SC Chemistry
GA 004OU
UT WOS:000308691800001
ER
PT J
AU Ichimura, AS
Zent, AP
Quinn, RC
Sanchez, MR
Taylor, LA
AF Ichimura, A. S.
Zent, A. P.
Quinn, R. C.
Sanchez, M. R.
Taylor, L. A.
TI Hydroxyl (OH) production on airless planetary bodies: Evidence from
H+/D+ ion-beam experiments
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE solar wind; hydroxyl; infrared; proton ion-beam; OH; lunar soil
ID SOLAR-WIND; LUNAR-SURFACE; MARE SOILS; MOON; HYDROGEN; IMPLANTATION;
REGOLITH; DEPOSITS; PROTONS; OH/H2O
AB The hypothesis that bombardment of lunar soil with solar-wind protons might form hydroxyl (OH) and perhaps HOH has been tested by experiments with Apollo 16 (highlands) and Apollo 17 (mare) soils. Pre-dried soils (500 degrees C) were bombarded with 1.1 key protons and deuterons and provide unambiguous evidence for the formation of OH or OD in both samples. This hypothesis further predicts the formation of hydroxyl (OH) on other airless planetary/asteroidal bodies, with a sufficient solar-wind flux. Deuteron implantation of unaltered lunar soils and a heat-treated plagioclase specimen cause simultaneous OH depletion and OD formation. Ion bombardment of lunar soils simulates the dynamic process of hydroxyl formation and may also deplete intrinsic OH, thereby effectively contributing to the day/night, diurnal variability of OH reported by Sunshine et al. (2009). Our results emphasize the need to use lunar soils with space-weathered exteriors in laboratory simulations of the solar wind. Infrared spectra of hydrogen ion-beam implanted soils are similar to spectra obtained at RELAB (Brown Univ.) and to those observed by remote sensing confirming the solar-wind hypothesis. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Ichimura, A. S.; Sanchez, M. R.] San Francisco State Univ, Dept Chem & Biochem, San Francisco, CA 94132 USA.
[Zent, A. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Quinn, R. C.] SETI Inst, Mountain View, CA 94043 USA.
[Taylor, L. A.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
RP Ichimura, AS (reprint author), San Francisco State Univ, Dept Chem & Biochem, 1600 Holloway Ave, San Francisco, CA 94132 USA.
EM ichimura@sfsu.edu; Aaron.P.Zent@nasa.gov
FU NASA [NNX11AN74A, NNX11AG58G]; NSF [064814, 0821619]
FX This research was supported by NASA Grants NNX11AN74A (ASI), LASER WBS
element 964946.02.06.01.98 (APZ), NNX11AG58G (LAT), and NSF awards
064814 and 0821619 (ASI). This research uses spectra acquired by C.M.
Pieters with the NASA-RELAB facility at Brown University. The Planetary
Geosciences Institute at UT provided partial support for LAT.
NR 49
TC 15
Z9 16
U1 2
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD SEP
PY 2012
VL 345
BP 90
EP 94
DI 10.1016/j.epsl.2012.06.027
PG 5
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 002HN
UT WOS:000308522800010
ER
PT J
AU Powell, SW
Houze, RA
Kumar, A
McFarlane, SA
AF Powell, Scott W.
Houze, Robert A., Jr.
Kumar, Anil
McFarlane, Sally A.
TI Comparison of Simulated and Observed Continental Tropical Anvil Clouds
and Their Radiative Heating Profiles
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID RESOLVING MODEL SIMULATIONS; MESOSCALE CONVECTIVE SYSTEMS; AFRICAN
SQUALL LINES; WEST-AFRICAN; STRATIFORM PRECIPITATION; CLIMATE MODELS;
ACCURATE PARAMETERIZATION; DOPPLER RADAR; CIRRUS CLOUDS; ICE CLOUDS
AB Vertically pointing millimeter-wavelength radar observations of anvil clouds extending from mesoscale convective systems (MCSs) that pass over an Atmospheric Radiation Measurement Program (ARM) field site in Niamey, Niger, are compared to anvil structures generated by the Weather Research and Forecasting (WRF) mesoscale model using six different microphysical schemes. The radar data provide the statistical distribution of the radar reflectivity values as a function of height and anvil thickness. These statistics are compared to the statistics of the modeled anvil cloud reflectivity at all altitudes. Requiring the model to be statistically accurate at all altitudes is a stringent test of the model performance. The typical vertical profile of radiative heating in the anvil clouds is computed from the radar observations. Variability of anvil structures from the different microphysical schemes provides an estimate of the inherent uncertainty in anvil radiative heating profiles. All schemes underestimate the optical thickness of thin anvils and cirrus, resulting in a bias of excessive net anvil heating in all of the simulations.
C1 [Powell, Scott W.; Houze, Robert A., Jr.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Kumar, Anil] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Kumar, Anil] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[McFarlane, Sally A.] Pacific NW Natl Lab, Climate Phys Grp, Richland, WA 99352 USA.
RP Powell, SW (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA.
EM spowell@atmos.uw.edu
FU DOE [DE-SC0001164/ER-64752]
FX This work was supported by DOE Grant DE-SC0001164/ER-64752. Stacy
Brodzik provided technical support and data management. Beth Tully
provided graphics and editorial assistance. The authors thank Alain
Protat and two anonymous reviewers for their constructive comments on
the manuscript.
NR 64
TC 15
Z9 15
U1 3
U2 15
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2012
VL 69
IS 9
BP 2662
EP 2681
DI 10.1175/JAS-D-11-0251.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 999AB
UT WOS:000308280400003
ER
PT J
AU Yan, Y
Yue, Y
Huang, H
Yang, JY
Chitgarha, MR
Ahmed, N
Tur, M
Dolinar, SJ
Willner, AE
AF Yan, Yan
Yue, Yang
Huang, Hao
Yang, Jeng-Yuan
Chitgarha, Mohammad R.
Ahmed, Nisar
Tur, Moshe
Dolinar, Samuel. J.
Willner, Alan E.
TI Efficient generation and multiplexing of optical orbital angular
momentum modes in a ring fiber by using multiple coherent inputs
SO OPTICS LETTERS
LA English
DT Article
ID LIGHT; BEAMS
AB We propose an approach to efficiently generate and multiplex optical orbital angular momentum (OAM) modes in a fiber with a ring refractive index profile by using multiple coherent inputs from a Gaussian mode. By controlling the phase relationship of the multiple inputs, one can selectively generate OAM modes of different states l. By controlling both the amplitude and phase of the multiple inputs, multiple OAM modes can be generated simultaneously without additional loss coming from multiplexing. We show, by simulation, the generation of OAM modes (OAM state [l] < 3) with mode purity greater than 99%. The power loss of generating and multiplexing seven modes is about 35%. A transmitter for an OAM-based mode-division multiplexing system is proposed based on the discrete Fourier transform between the data carried by the multiple inputs and the data carried by the OAM modes. The experimental implementation of the proposed approach could be achieved by integrating ring fiber, multicore fiber, and photonic integrated circuit technology. (c) 2012 Optical Society of America
C1 [Yan, Yan; Yue, Yang; Huang, Hao; Yang, Jeng-Yuan; Chitgarha, Mohammad R.; Ahmed, Nisar; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
[Tur, Moshe] Tel Aviv Univ, Sch Elect Engn, IL-69978 Tel Aviv, Israel.
[Dolinar, Samuel. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yan, Y (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
EM yanyan@usc.edu
RI Yue, Yang/A-3357-2012
FU Defense Advanced Research Projects Agency under the InPho program
FX We acknowledge the support of Defense Advanced Research Projects Agency
under the InPho program.
NR 12
TC 20
Z9 21
U1 1
U2 35
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
J9 OPT LETT
JI Opt. Lett.
PD SEP 1
PY 2012
VL 37
IS 17
BP 3645
EP 3647
PG 3
WC Optics
SC Optics
GA 003GD
UT WOS:000308595300057
PM 22940977
ER
PT J
AU Gudipati, MS
Yang, R
AF Gudipati, Murthy S.
Yang, Rui
TI IN-SITU PROBING OF RADIATION-INDUCED PROCESSING OF ORGANICS IN
ASTROPHYSICAL ICE ANALOGS-NOVEL LASER DESORPTION LASER IONIZATION
TIME-OF-FLIGHT MASS SPECTROSCOPIC STUDIES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; astrochemistry; evolution; methods: laboratory; planets
and satellites: surfaces; radiation mechanisms: non-thermal
ID POLYCYCLIC AROMATIC-HYDROCARBONS; INTERSTELLAR ICE;
ULTRAVIOLET-IRRADIATION; AMINO-ACIDS; WATER ICE; OPTICAL SPECTROSCOPY;
PROTOPLANETARY DISKS; FACILE GENERATION; RADICAL CATIONS; PAH CATIONS
AB Understanding the evolution of organic molecules in ice grains in the interstellar medium (ISM) under cosmic rays, stellar radiation, and local electrons and ions is critical to our understanding of the connection between ISM and solar systems. Our study is aimed at reaching this goal of looking directly into radiation-induced processing in these ice grains. We developed a two-color laser-desorption laser-ionization time-of-flight mass spectroscopic method (2C-MALDI-TOF), similar to matrix-assisted laser desorption and ionization time-of-flight (MALDI-TOF) mass spectroscopy. Results presented here with polycyclic aromatic hydrocarbon (PAH) probe molecules embedded in water-ice at 5 K show for the first time that hydrogenation and oxygenation are the primary chemical reactions that occur in astrophysical ice analogs when subjected to Ly alpha radiation. We found that hydrogenation can occur over several unsaturated bonds and the product distribution corresponds to their stabilities. Multiple hydrogenation efficiency is found to be higher at higher temperatures (100 K) compared to 5 K-close to the interstellar ice temperatures. Hydroxylation is shown to have similar efficiencies at 5 K or 100 K, indicating that addition of O atoms or OH radicals to pre-ionized PAHs is a barrierless process. These studies-the first glimpses into interstellar ice chemistry through analog studies-show that once accreted onto ice grains PAHs lose their PAH spectroscopic signatures through radiation chemistry, which could be one of the reason for the lack of PAH detection in interstellar ice grains, particularly the outer regions of cold, dense clouds or the upper molecular layers of protoplanetary disks.
C1 [Gudipati, Murthy S.; Yang, Rui] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gudipati, Murthy S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
RP Gudipati, MS (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gudipati@jpl.nasa.gov; ryang73@ustc.edu
RI Gudipati, Murthy/F-7575-2011
FU JPL's DRDF; JPL; NASA Spitzer Science Center; NASA through Rosetta US
Science Team; NASA Astrobiology Institute Node "Icy Worlds"
FX This research was enabled through partial funding from JPL's DRDF and
R&TD funding for infrastructure of the "Ice Spectroscopy Laboratory" at
JPL, NASA Spitzer Science Center, NASA funding through Rosetta US
Science Team, and NASA Astrobiology Institute Node "Icy Worlds". 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 49
TC 19
Z9 19
U1 3
U2 33
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 SEP 1
PY 2012
VL 756
IS 1
AR L24
DI 10.1088/2041-8205/756/1/L24
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 996HF
UT WOS:000308074800024
ER
PT J
AU Misra, V
Pantina, P
Chan, SC
DiNapoli, S
AF Misra, Vasubandhu
Pantina, P.
Chan, S. C.
DiNapoli, S.
TI A comparative study of the Indian summer monsoon hydroclimate and its
variations in three reanalyses
SO CLIMATE DYNAMICS
LA English
DT Article
DE Monsoon; Intraseasonal; Interannual
ID ATMOSPHERE COUPLING EXPERIMENT; DATA ASSIMILATION SYSTEM; SOUTH ASIAN
MONSOON; INTERANNUAL VARIABILITY; LAND-SURFACE; GLOBAL PRECIPITATION;
SOIL-MOISTURE; GREAT-PLAINS; WARM-SEASON; RAINFALL
AB This study examines the Indian summer monsoon hydroclimate in the National Centers for Environmental Prediction (NCEP)-Department of Energy (DOE) Reanalysis (R2), the Climate Forecast System Reanalysis (CFSR), and the Modern Era Retrospective-Analysis for Research and Applications (MERRA). The three reanalyses show significant differences in the climatology of evaporation, low-level winds, and precipitable water fields over India. For example, the continental evaporation is significantly less in CFSR compared to R2 and MERRA. Likewise the mean boreal summer 925 hPa westerly winds in the northern Indian Ocean are stronger in R2. Similarly the continental precipitable water in R2 is much less while it is higher and comparable in MERRA and CFSR. Despite these climatological differences between the reanalyses, the climatological evaporative sources for rain events over central India show some qualitative similarities. Major differences however appear when interannual variations of the Indian summer monsoon are analyzed. The anomalous oceanic sources of moisture from the adjacent Bay of Bengal and Arabian Sea play a significant role in determining the wet or dry year of the Indian monsoon in CFSR. However in R2 the local evaporative sources from the continental region play a more significant role. We also find that the interannual variability of the evaporative sources in the break spells of the intraseasonal variations of the Indian monsoon is stronger than in the wet spells. We therefore claim that instead of rainfall, evaporative sources may be a more appropriate metric to observe the relationship between the seasonal monsoon strength and intraseasonal activity. These findings are consistent across the reanalyses and provide a basis to improve the predictability of intraseasonal variability of the Indian monsoon. This study also has a bearing on improving weather prediction for tropical cyclones in that we suggest targeting enhanced observations in the Bay of Bengal (where it is drawing the most moisture from) for improved analysis during active spells of the intraseasonal variability of the Indian monsoon. The analysis suggests that the land-atmosphere interactions contribute significant uncertainty to the Indian monsoon in the reanalyses, which is consistent with the fact that most of the global reanalyses do not assimilate any land-surface data because the data are not available. Therefore, the land-atmosphere interaction in the reanalyses is highly dependent on the land-surface model and it's coupling with the atmospheric model.
C1 [Misra, Vasubandhu] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Misra, Vasubandhu; DiNapoli, S.] Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA.
[Pantina, P.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Pantina, P.] NASA GSFC, Cloud & Radiat Lab, Greenbelt, MD USA.
[Chan, S. C.] Newcastle Univ, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Chan, S. C.] Met Off Hadley Ctr, Exeter, Devon, England.
RP Misra, V (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
EM vmisra@fsu.edu; steven.chan@metoffice.gov.uk
FU NOAA [NA070AR4310221]; USDA
FX The authors would like to acknowledge the expert guidance of Kathy
Fearon of COAPS for her editorial corrections on an earlier version of
the manuscript. We acknowledge the resources of the Computational and
Information Systems Laboratory of NCAR to obtain some of the
observational datasets used for verification in this study. We also
thank Dr. Paul Dirmeyer of Center for Ocean, Land and Atmosphere Studies
(COLA) for sharing the Fortran code of the back trajectory program. The
useful review comments and suggestions of three anonymous reviewers on
an earlier version of the manuscript is also acknowledged. This work is
supported by NOAA grant NA070AR4310221 and the USDA.
NR 71
TC 15
Z9 15
U1 0
U2 17
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
J9 CLIM DYNAM
JI Clim. Dyn.
PD SEP
PY 2012
VL 39
IS 5
SI SI
BP 1149
EP 1168
DI 10.1007/s00382-012-1319-y
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 995BP
UT WOS:000307981900009
ER
PT J
AU Narock, T
Fox, P
AF Narock, Thomas
Fox, Peter
TI From science to e-Science to Semantic e-Science: A Heliophysics case
study
SO COMPUTERS & GEOSCIENCES
LA English
DT Review
DE Semantic e-Science; Semantic Web; Ontology; Provenance
ID ONTOLOGY; FIELD
AB The past few years have witnessed unparalleled efforts to make scientific data web accessible. The Semantic Web has proven invaluable in this effort; however, much of the literature is devoted to system design, ontology creation, and trials and tribulations of current technologies. In order to fully develop the nascent field of Semantic e-Science we must also evaluate systems in real-world settings. We describe a case study within the field of Heliophysics and provide a comparison of the evolutionary stages of data discovery, from manual to semantically enable. We describe the socio-technical implications of moving toward automated and intelligent data discovery. In doing so, we highlight how this process enhances what is currently being done manually in various scientific disciplines. Our case study illustrates that Semantic e-Science is more than just semantic search. The integration of search with web services, relational databases, and other cyberinfrastructure is a central tenet of our case study and one that we believe has applicability as a generalized research area within Semantic e-Science. This case study illustrates a specific example of the benefits, and limitations, of semantically replicating data discovery. We show examples of significant reductions in time and effort enable by Semantic e-Science; yet, we argue that a "complete" solution requires integrating semantic search with other research areas such as data provenance and web services. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Narock, Thomas] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
[Narock, Thomas] Adnet Syst Inc, Rockville, MD USA.
[Fox, Peter] Rensselaer Polytech Inst, Troy, NY 12181 USA.
RP Narock, T (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Code 672, Greenbelt, MD 20771 USA.
EM Thomas.W.Narock@nasa.gov
OI Fox, Peter/0000-0002-1009-7163; Narock, Tom/0000-0002-9785-4496
NR 55
TC 5
Z9 5
U1 0
U2 24
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD SEP
PY 2012
VL 46
BP 248
EP 254
DI 10.1016/j.cageo.2011.11.018
PG 7
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 994IN
UT WOS:000307924200029
ER
PT J
AU Marthews, TR
Malhi, Y
Girardin, CAJ
Espejo, JES
Aragao, LEOC
Metcalfe, DB
Rapp, JM
Mercado, LM
Fisher, RA
Galbraith, DR
Fisher, JB
Salinas-Revilla, N
Friend, AD
Restrepo-Coupe, N
Williams, RJ
AF Marthews, Toby R.
Malhi, Yadvinder
Girardin, Cecile A. J.
Silva Espejo, Javier E.
Aragao, Luiz E. O. C.
Metcalfe, Daniel B.
Rapp, Joshua M.
Mercado, Lina M.
Fisher, Rosie A.
Galbraith, David R.
Fisher, Joshua B.
Salinas-Revilla, Norma
Friend, Andrew D.
Restrepo-Coupe, Natalia
Williams, Richard J.
TI Simulating forest productivity along a neotropical elevational transect:
temperature variation and carbon use efficiency
SO GLOBAL CHANGE BIOLOGY
LA English
DT Review
DE tropical forest production; JULES model; field measurements; maintenance
respiration; Peru; Brazil
ID NET PRIMARY PRODUCTIVITY; WET TROPICAL MOUNTAINS; AMAZONIAN RAIN-FOREST;
BASIN-WIDE VARIATIONS; ALTITUDINAL VARIATION; LITTER DECOMPOSITION;
PHYSICAL-PROPERTIES; PLANT RESPIRATION; MODEL DESCRIPTION; VEGETATION
MODEL
AB A better understanding of the mechanisms controlling the magnitude and sign of carbon components in tropical forest ecosystems is important for reliable estimation of this important regional component of the global carbon cycle. We used the JULES vegetation model to simulate all components of the carbon balance at six sites along an Andes-Amazon transect across Peru and Brazil and compared the results to published field measurements. In the upper montane zone the model predicted a lack of forest vegetation, indicating a need for better parameterization of the responses of cloud forest vegetation within the model. In the lower montane and lowland zones simulated ecosystem productivity and respiration were predicted with reasonable accuracy, although not always within the error bounds of the observations. Model-predicted carbon use efficiency in this transect surprisingly did not increase with elevation, but remained close to the temperate value 0.5. Upper montane forests were predicted to allocate similar to 50% of carbon fixation to biomass maintenance and growth, despite available measurements showing that they only allocate similar to 33%. This may be explained by elevational changes in the balance between growth and maintenance respiration within the forest canopy, as controlled by both temperature- and pressure-mediated processes, which is not yet well represented in current vegetation models.
C1 [Marthews, Toby R.; Malhi, Yadvinder; Girardin, Cecile A. J.; Galbraith, David R.; Salinas-Revilla, Norma] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England.
[Silva Espejo, Javier E.; Salinas-Revilla, Norma] Univ Nacl San Antonio Abad Cusco, Cuzco, Peru.
[Aragao, Luiz E. O. C.; Mercado, Lina M.] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4RJ, Devon, England.
[Metcalfe, Daniel B.] Sveriges Lantbruksuniv, S-90183 Umea, Sweden.
[Rapp, Joshua M.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA.
[Mercado, Lina M.] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England.
[Fisher, Rosie A.] Los Alamos Natl Lab, Earth & Environm Sci Div, Los Alamos, NM 87545 USA.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Friend, Andrew D.] Univ Cambridge, Dept Geog, Cambridge CB2 3EN, England.
[Restrepo-Coupe, Natalia] Univ Technol Sydney, Broadway, NSW 2007, Australia.
[Williams, Richard J.] Microsoft Res, Computat Ecol & Environm Sci Grp, Cambridge CB3 0FB, England.
RP Marthews, TR (reprint author), Univ Oxford, Sch Geog & Environm, Environm Change Inst, S Parks Rd, Oxford OX1 3QY, England.
EM Toby.Marthews@ouce.ox.ac.uk
RI aragao, luiz/G-8387-2012; Rapp, Joshua/C-4061-2013; Fisher,
Rosie/E-7746-2013; MARTHEWS, TOBY/H-6264-2014; Restrepo-Coupe,
Natalia/C-3507-2015; Salinas, Norma/K-8960-2015;
OI aragao, luiz/0000-0002-4134-6708; Rapp, Joshua/0000-0002-7767-5837;
MARTHEWS, TOBY/0000-0003-3727-6468; Restrepo-Coupe,
Natalia/0000-0003-3921-1772; Salinas, Norma/0000-0001-9941-2109; Fisher,
Joshua/0000-0003-4734-9085
FU UK NERC Amazon Integrated Carbon Analysis (AMAZONICA) consortium grant
[NE/F005997/1]
FX This study is a product of the Andes Biodiversity and Ecosystem Research
Group (ABERG, http://darwin.winston.wfu.edu/andes/) and has drawn
heavily on collaborators, infrastructure and data sources available
through ABERG as well as RAINFOR
(http://www.geog.leeds.ac.uk/projects/rainfor/). We are indebted to the
Gordon and Betty Moore Foundation (grant to RAINFOR) and Microsoft
Research, the Jackson Foundation and Oxford Martin School (grants to Y.
Malhi) and L. Mercado was supported by the UK NERC Amazon Integrated
Carbon Analysis (AMAZONICA) consortium grant (NE/F005997/1). Thanks to
J. Fisher and I. Torres for use of canopy height data from their
fertilization plots in Peru and to J. Fisher and M. Unger for
unpublished leaf nitrogen data from Ecuador. We thank the Asociacion
para la Conservacion de la Cuenca Amazonica (ACCA) for the use of the
Wayqecha field station in 2010. Also thanks to D. Clark and M. van Oijen
for very useful correspondence and to the Oxford Supercomputing Centre
for the use of their resources for some of our simulation runs.
NR 123
TC 12
Z9 14
U1 3
U2 83
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD SEP
PY 2012
VL 18
IS 9
BP 2882
EP 2898
DI 10.1111/j.1365-2486.2012.02728.x
PG 17
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 984WH
UT WOS:000307222700019
PM 24501065
ER
PT J
AU Scharf, DP
AF Scharf, Daniel P.
TI Analytic Yaw-Pitch Steering for Side-Looking SAR With Numerical Roll
Algorithm for Incidence Angle
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Attitude control; synthetic aperture radar (SAR)
AB In side-looking synthetic aperture radars (SARs), the rotation of the Earth introduces a corrupting residual Doppler shift. Recently, methods using both yaw and pitch maneuvers have been introduced to cancel residual Doppler. In this paper, the condition for zero residual Doppler independent of a coordinate system is used as a starting point to derive formulas for yaw-then-pitch steering angles that achieve zero residual Doppler for strip-mode SAR. The advantage is that the resulting formulas are analytic in the position and velocity of the radar vehicle. In addition, the magnitude of residual Doppler due to both the offset of the radar phase center from the vehicle center of mass and an ellipsoidal Earth is bounded. To take advantage of the final degree of freedom in roll, a bisection-based roll algorithm is presented that achieves a desired radar incidence angle. The algorithm assumes an ellipsoidal Earth but can incorporate digital elevation and geoid models. Finally, numerical examples illustrate yaw-then-pitch steering, the sensitivity of these angles to the specific orbit, and calculation of the roll angle.
C1 CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Pasadena, CA 91109 USA.
RP Scharf, DP (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Daniel.P.Scharf@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was conducted at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. The author would like to thank Dr.
S. Shaffer of JPL for clarifying some radar concepts.
NR 15
TC 6
Z9 6
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2012
VL 50
IS 9
BP 3587
EP 3594
DI 10.1109/TGRS.2012.2183375
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 996PY
UT WOS:000308105600026
ER
PT J
AU Yim, KB
Yim, J
AF Yim, Kyung Bin
Yim, John
TI Dynamic Behavior of Overhung Rotors Subjected to Axial Forces
SO INTERNATIONAL JOURNAL OF PRECISION ENGINEERING AND MANUFACTURING
LA English
DT Article
DE Axial force; Dynamic behavior; Overhung rotor; Transfer matrix method
ID STABILITY; LOADS; COLUMNS; SHAFT; MASS
AB The dynamic behavior of a flexible shaft with a disk subjected to axial forces has been studied by employing the transfer matrix approach. The conventional transfer matrix was modified to include the applied axial force, and then integrated into a computer program to investigate the effect of the load force on the stability and the natural frequencies of overhung rotor systems. Two overhung rotor systems are considered. One is the cantilevered rotor and the other is the overhung rotor with an intermediate support. The gyroscopic effect of the rotor strongly influences the dynamic behavior of the shaft-disk system under axial forces not only by increasing the critical force for the stability but also by changing the instability type from divergence to flutter.
C1 [Yim, Kyung Bin] Dongyang Mirae Univ, Sch Mech Engn, Seoul 152714, South Korea.
[Yim, John] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Yim, KB (reprint author), Dongyang Mirae Univ, Sch Mech Engn, 62-160 Gochuk Dong, Seoul 152714, South Korea.
EM kbyim@dongyang.ac.kr
FU Dongyang Mirae University
FX This work was supported by Dongyang Mirae University.
NR 9
TC 3
Z9 4
U1 2
U2 6
PU KOREAN SOC PRECISION ENG
PI SEOUL
PA RM 306, KWANGMYUNG BLDG, 5-4 NONHYUN-DONG, KANGNAM-GU, SEOUL, 135-010,
SOUTH KOREA
SN 2234-7593
J9 INT J PRECIS ENG MAN
JI Int. J. Precis. Eng. Manuf.
PD SEP
PY 2012
VL 13
IS 9
BP 1575
EP 1580
DI 10.1007/s12541-012-0207-z
PG 6
WC Engineering, Manufacturing; Engineering, Mechanical
SC Engineering
GA 001FX
UT WOS:000308447100010
ER
PT J
AU Kuai, L
Wunch, D
Shia, RL
Connor, B
Miller, C
Yung, Y
AF Kuai, Le
Wunch, Debra
Shia, Run-Lie
Connor, Brian
Miller, Charles
Yung, Yuk
TI Vertically constrained CO2 retrievals from TCCON measurements
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE TCCON; Carbon dioxide; Retrieval
ID FOURIER-TRANSFORM SPECTROMETRY; COLUMN OBSERVING NETWORK; GREENHOUSE
GASES; ATMOSPHERIC CO2; CARBON; CALIBRATION; SPECTRA; GOSAT; PROFILES;
SYSTEM
AB Partial column-averaged carbon dioxide (CO2) mixing ratio in three tropospheric layers has been retrieved from Total Carbon Column Observing Network (TCCON) spectra in the 1.6 mu m CO2 absorption band. Information analysis suggests that a measurement with similar to 60 absorption lines provides three or more pieces of independent information, depending on the signal-to-noise ratio and solar zenith angle. This has been confirmed by retrievals based on synthetic data. Realistic retrievals for both total and partial column-averaged CO2 over Park Falls, Wisconsin on July 12, 15, and August 14, 2004, agree with aircraft measurements. Furthermore, the retrieved total column averages are always underestimated by less than 1%. The results above provide a basis for CO2 profile retrievals using ground-based observations in the near-infrared region. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Kuai, Le; Wunch, Debra; Shia, Run-Lie; Yung, Yuk] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Connor, Brian] BC Consulting Ltd, Alexandra 9320, New Zealand.
[Miller, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Kuai, L (reprint author), CALTECH, Div Geol & Planetary Sci, MC 150-21, Pasadena, CA 91125 USA.
EM kl@gps.caltech.edu
FU NASA [JPL.1382974, NNX11AG01G]
FX This research is supported in part by the Orbiting Carbon Observatory 2
(OCO-2) project, a NASA Earth System Science Pathfinder (ESSP) mission
and Project JPL.1382974 to the California Institute of Technology.
Support for TCCON and operations at Park Falls Wisconsin are provided by
a grant from NASA to the California Institute of Technology
(NNX11AG01G). We would like to thank Gretchen Keppel Aleks, Mimi
Gerstell, Vijay Natraj, Sally Newman, Jack Margolis, Xi Zhang, King-Fai
Li, and Michael Line for useful discussions and comments on the paper.
Special thanks are given to G. Toon and P. Wennberg for making available
their code and data, and for valuable discussions.
NR 39
TC 8
Z9 8
U1 0
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD SEP
PY 2012
VL 113
IS 14
BP 1753
EP 1761
DI 10.1016/j.jqsrt.2012.04.024
PG 9
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 976VN
UT WOS:000306615400002
ER
PT J
AU Zakharova, NT
Videen, G
Khlebtsov, NG
AF Zakharova, Nadezhda T.
Videen, Gorden
Khlebtsov, Nikolai G.
TI Comprehensive T-matrix reference database: A 2009-2011 update
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electromagnetic scattering; T-matrix method; Nonspherical particles;
Many-particle aggregates
ID LIGHT ABSORBING CARBON; DISCRETE DIPOLE APPROXIMATION; LORENZ-MIE
THEORY; OPTICAL-PROPERTIES; ELECTROMAGNETIC SCATTERING; NONSPHERICAL
PARTICLES; METAL NANOPARTICLES; FAR-FIELD; RADIATIVE PROPERTIES;
MULTIPLE-SCATTERING
AB The T-matrix method is one of the most versatile and efficient theoretical techniques widely used for the computation of electromagnetic scattering by single and composite particles, discrete random media, and particles in the vicinity of an interface separating two half-spaces with different refractive indices. This paper presents an update to the comprehensive database of peer-reviewed T-matrix publications compiled by us previously and includes the publications that appeared since 2009. It also lists several earlier publications not included in the original database. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Zakharova, Nadezhda T.] NASA, Trinnovim, Goddard Inst Space Studies, New York, NY 10025 USA.
[Videen, Gorden] USA, Res Lab, AMSRL IS EE, Adelphi, MD 20783 USA.
[Khlebtsov, Nikolai G.] Russian Acad Sci, Inst Biochem & Physiol Plants & Microorganisms, Saratov 410015, Russia.
RP Zakharova, NT (reprint author), NASA, Trinnovim, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM nadezhda.zakharova@nasa.gov
RI Khlebtsov, Nikolai/D-6199-2017; Pylaev, Timofey/A-8401-2016;
OI Pylaev, Timofey/0000-0002-2701-3333; Khlebtsov,
Nikolai/0000-0002-2055-7784
FU NASA
FX We thank Josefina Mora and Zoe Wai for helping to obtain copies of
publications that were not readily accessible. This project was
sponsored by NASA.
NR 294
TC 13
Z9 13
U1 1
U2 33
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD SEP
PY 2012
VL 113
IS 14
BP 1844
EP 1852
DI 10.1016/j.jqsrt.2012.04.009
PG 9
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 976VN
UT WOS:000306615400008
ER
PT J
AU Marshak, A
Knyazikhin, Y
Chiu, JC
Wiscombe, WJ
AF Marshak, Alexander
Knyazikhin, Yuri
Chiu, J. Christine
Wiscombe, Warren J.
TI On spectral invariance of single scattering albedo for water droplets
and ice crystals at weakly absorbing wavelengths (vol 113, pg 715, 2012)
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Correction
C1 [Marshak, Alexander; Wiscombe, Warren J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Knyazikhin, Yuri] Boston Univ, Boston, MA 02215 USA.
[Chiu, J. Christine] Univ Reading, Dept Meteorol, Reading, Berks, England.
RP Marshak, A (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
EM alexander.marshak@nasa.gov
RI Chiu, Christine/E-5649-2013; Wiscombe, Warren/D-4665-2012
OI Chiu, Christine/0000-0002-8951-6913; Wiscombe,
Warren/0000-0001-6844-9849
NR 1
TC 0
Z9 0
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD SEP
PY 2012
VL 113
IS 14
BP 1853
EP 1853
DI 10.1016/j.jqsrt.2012.05.008
PG 1
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 976VN
UT WOS:000306615400009
ER
PT J
AU Sun, GS
Tou, JC
Reiss-Bubenheim, DA
Hill, EL
Liittschwager, KW
Girten, BE
Pena-Yewkukhiw, E
AF Sun, Gwo-Shing
Tou, Janet C.
Reiss-Bubenheim, Debra A.
Hill, Esther L.
Liittschwager, Kurt W.
Girten, Beverly E.
Pena-Yewkukhiw, Eugenia
TI Oxidative and nutrient stability of a standard rodent spaceflight diet
during long-term storage
SO LAB ANIMAL
LA English
DT Article
ID PERFORMANCE; CHEMISTRY; LIPIDS; ACID
AB The National Aeronautics and Space Administration's standard spaceflight diet for rodents is the nutrient-upgraded rodent food bar (NuRFB). The shelf life of the NuRFB needs to be determined in order to avoid malnutrition of rodents and confounding of research results resulting from nutritional deficiency. The authors compared the oxidative and nutrient stability of NuRFBs stored at either ambient temperature (26 degrees C) or at refrigeration temperature (4 degrees C) for use in long-term rodent feeding experiments. After 0, 3, 6, 9 and 12 months (mo) of storage, lipid oxidation, fatty acid composition and amounts of specific vitamins and amino acids in NuRFBs were analyzed. No oxidative rancidity developed in NuRFBs stored at 4 degrees C for up to 12 mo, but NuRFBs stored at 26 degrees C for 6 mo developed oxidative rancidity and had reduced amounts of gamma-linolenic acid (18:3n-6). Despite loss of vitamin E, vitamin A and thiamin after storage at 26 degrees C for 12 mo, vitamin levels in NuRFBs remained at or above the levels recommended for optimal rodent health. The amino acid profile of NuRFBs was unaffected by storage at 4 degrees C or 26 degrees C for 12 mo. The results suggest that NuRFBs stored at 4 degrees C for up to 12 mo and NuRFBs stored at 26 degrees C for up to 6 mo provide suitable nutrition for rodents in long-term experiments.
C1 [Sun, Gwo-Shing; Hill, Esther L.; Liittschwager, Kurt W.] Lockheed Martin Explorat & Sci, Moffett Field, CA USA.
[Tou, Janet C.] W Virginia Univ, Div Anim & Nutr Sci, Morgantown, WV 26506 USA.
[Reiss-Bubenheim, Debra A.; Girten, Beverly E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pena-Yewkukhiw, Eugenia] W Virginia Univ, Div Plant & Soil Sci, Morgantown, WV 26506 USA.
RP Sun, GS (reprint author), Lockheed Martin Explorat & Sci, Moffett Field, CA USA.
EM gwo-shing.sun-1@nasa.gov
NR 25
TC 2
Z9 2
U1 0
U2 1
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 0093-7355
J9 LAB ANIMAL
JI Lab Anim.
PD SEP
PY 2012
VL 41
IS 9
BP 252
EP +
PG 8
WC Veterinary Sciences
SC Veterinary Sciences
GA 998XY
UT WOS:000308274900017
PM 22914028
ER
PT J
AU Gozdziewski, K
Nasiroglu, I
Slowikowska, A
Beuermann, K
Kanbach, G
Gauza, B
Maciejewski, AJ
Schwarz, R
Schwope, AD
Hinse, TC
Haghighipour, N
Burwitz, V
Slonina, M
Rau, A
AF Gozdziewski, Krzysztof
Nasiroglu, Ilham
Slowikowska, Aga
Beuermann, Klaus
Kanbach, Gottfried
Gauza, Bartosz
Maciejewski, Andrzej J.
Schwarz, Robert
Schwope, Axel D.
Hinse, Tobias C.
Haghighipour, Nader
Burwitz, Vadim
Slonina, Mariusz
Rau, Arne
TI On the HU Aquarii planetary system hypothesis
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; methods: numerical; techniques: photometric;
celestial mechanics; planets and satellites: dynamical evolution and
stability
AB In this paper, we investigate the eclipse timing of the polar binary HU?Aquarii that has been observed for almost two decades. Recently, Qian et al. attributed large (OC) deviations between the eclipse ephemeris and observations to a compact system of two massive Jovian companions. We improve the Keplerian, kinematic model of the light travel time effect and re-analyse the whole currently available data set. We add almost 60 new, yet unpublished, mostly precision light curves obtained using the time high-resolution photopolarimeter Optical Timing Analyzer (OPTIMA), as well as photometric observations performed at the Monitoring Network of Telescopes/North, Physics Innovations Robotic Astronomical Telescope Explorer and Carlos Sanchez Telescope. We determine new mid-egress times with a mean uncertainty at the level of 1?s or better. We claim that because the observations that currently exist in the literature are non-homogeneous with respect to spectral windows (ultraviolet, X-ray, visual and polarimetric mode) and the reported mid-egress measurements errors, they may introduce systematics that affect orbital fits. Indeed, we find that the published data, when taken literally, cannot be explained by any unique solution. Many qualitatively different and best-fit two-planet configurations, including self-consistent, Newtonian N-body solutions may be able to explain the data. However, using high-resolution, precision OPTIMA light curves, we find that the (OC) deviations are best explained by the presence of a single circumbinary companion orbiting at a distance of similar to 4.5?au with a small eccentricity and having similar to 7 Jupiter masses. This object could be the next circumbinary planet detected from the ground, similar to the announced companions around close binaries HW?Vir, NN?Ser, UZ?For, DP?Leo, FS?Aur or SZ?Her, and planets of this type around Kepler-16, Kepler-34 and Kepler-35.
C1 [Gozdziewski, Krzysztof; Slonina, Mariusz] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland.
[Nasiroglu, Ilham; Kanbach, Gottfried; Burwitz, Vadim; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Nasiroglu, Ilham] Cukurova Univ, Dept Phys, TR-01330 Adana, Turkey.
[Slowikowska, Aga; Maciejewski, Andrzej J.] Univ Zielona Gora, Kepler Inst Astron, PL-65265 Zielona Gora, Poland.
[Beuermann, Klaus] Univ Gottingen, Inst Astrophys, DE-37077 Gottingen, Germany.
[Gauza, Bartosz] Inst Astrofis Canarias IAC, E-38200 Tenerife, Spain.
[Gauza, Bartosz] Univ La Laguna ULL, Inst Astrofis, E-38206 Tenerife, Spain.
[Schwarz, Robert; Schwope, Axel D.] Leibniz Inst Astrophys AIP, D-14482 Potsdam, Germany.
[Hinse, Tobias C.] Korea Astron & Space Sci Inst KASI, Opt Astron Res Ctr, Taejon 305348, South Korea.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Burwitz, Vadim] Observ Astron Mallorca, Costitx 07144, Mallorca, Spain.
RP Gozdziewski, K (reprint author), Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland.
EM k.gozdziewski@astri.uni.torun.pl
RI Gozdziewski, Krzysztof/D-6291-2014
OI Gozdziewski, Krzysztof/0000-0002-8705-1577
FU Polish Ministry of Science and Higher Education [N/N203/402739]; POWIEW
project of the European Regional Development Fund in Innovative Economy
Programme [POIG.02.03.00-00-018/08]; EU FP6 Transfer of Knowledge
Project 'Astrophysics of Neutron Stars' [MKTD-CT-2006-042722];
Foundation for Polish Science [FNP HOM/2009/11B]; Marie Curie European
Reintegration Grant within the 7th European Community Framework
Programme [PERG05-GA-2009-249168]; KRCF Young Researcher Fellowship
Program at the Korea Astronomy and Space Science Institute; NASA
Astrobiology Institute at the Institute for Astronomy, University of
Hawaii [NNA09DA77A]; NASA/EXOB program [NNX09AN05G]; Alfried Krupp von
Bohlen und Halbach Foundation, Essen; Skinakas Observatory
FX We thank the anonymous referee for a review and comments that improved
the manuscript. We would like to thank Maciej Konacki (CAMK Torun) for a
discussion and a suggestion of the egress slopes test, as well as Anna
Zajczyk (CAMK, Torun), Andrzej Szary (UZG, Zielona Gora), Alex
Stefanescu, Martin Muhlegger, Helmut Steinle, Natalia Primak, Fritz
Schrey and Christian Straubmeier (all MPE) for their help with
observations. KG is supported by the Polish Ministry of Science and
Higher Education Grant No. N/N203/402739 and POWIEW project of the
European Regional Development Fund in Innovative Economy Programme
POIG.02.03.00-00-018/08. IN acknowledges support from the EU FP6
Transfer of Knowledge Project 'Astrophysics of Neutron Stars'
(MKTD-CT-2006-042722). AS would like to thank Bronek Rudak for his
support and discussions. She also acknowledges support from the
Foundation for Polish Science grant FNP HOM/2009/11B, as well as from
the Marie Curie European Reintegration Grant within the 7th European
Community Framework Programme (PERG05-GA-2009-249168). GK acknowledges
support from the EU FP6 Transfer of Knowledge Project ASTROCENTER
(MTKD-CT-2006-039965) and the kind hospitality of the Skinakas team at
UoC. BG thanks the Wide FastCam team for help in performing the
observations. Research by TCH is carried out under the KRCF Young
Researcher Fellowship Program at the Korea Astronomy and Space Science
Institute. NH acknowledges support from the NASA Astrobiology Institute
under Cooperative Agreement NNA09DA77A at the Institute for Astronomy,
University of Hawaii, and from NASA/EXOB program under grant NNX09AN05G.
We thank the Skinakas Observatory for their support and allocation of
telescope time. Skinakas Observatory is a collaborative project of the
University of Crete, the Foundation for Research and Technology -
Hellas, and the Max-Planck-Institute for Extraterrestrial Physics. This
paper is based on observations made with the TCS telescope operated on
the island of Tenerife by the Instituto de Astrofisica de Canarias in
the Spanish Teide Observatory. This work is based in part on data
obtained with the MONET, funded by the Alfried Krupp von Bohlen und
Halbach Foundation, Essen, and operated by the Georg-August-Universitat
Gottingen, the McDonald Observatory of the University of Texas at Austin
and the South African Astronomical Observatory.
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SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2012
VL 425
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BP 930
EP 949
DI 10.1111/j.1365-2966.2012.21341.x
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 993VQ
UT WOS:000307888300008
ER
PT J
AU Derekas, A
Szabo, GM
Berdnikov, L
Szabo, R
Smolec, R
Kiss, LL
Szabados, L
Chadid, M
Evans, NR
Kinemuchi, K
Nemec, JM
Seader, SE
Smith, JC
Tenenbaum, P
AF Derekas, A.
Szabo, Gy. M.
Berdnikov, L.
Szabo, R.
Smolec, R.
Kiss, L. L.
Szabados, L.
Chadid, M.
Evans, N. R.
Kinemuchi, K.
Nemec, J. M.
Seader, S. E.
Smith, J. C.
Tenenbaum, P.
TI Period and light-curve fluctuations of the Kepler Cepheid V1154 Cygni
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; planets and satellites: detection; stars:
individual: V1154 Cyg; stars: variables: Cepheids
ID GRAVITATIONAL LENSING EXPERIMENT.; OGLE-III CATALOG;
LARGE-MAGELLANIC-CLOUD; CLASSICAL CEPHEIDS; INITIAL CHARACTERISTICS;
CADENCE DATA; MODELS; PULSATIONS; STARS; POLARIS
AB We present a detailed period analysis of the bright Cepheid-type variable star V1154 Cygni (V1154 Cyg; V = 9.1?mag, P 4.9?d) based on almost 600?d of continuous observations by the Kepler space telescope. The data reveal significant cycle-to-cycle fluctuations in the pulsation period, indicating that classical Cepheids may not be as accurate astrophysical clocks as commonly believed: regardless of the specific points used to determine the O - C values, the cycle lengths show a scatter of 0.0150.02?d over 120 cycles covered by the observations. A very slight correlation between the individual Fourier parameters and the O - C values was found, suggesting that the O - C variations might be due to the instability of the light-curve shape. Random-fluctuation tests revealed a linear trend up to a cycle difference 15, but for long term, the period remains around the mean value. We compare the measurements with simulated light curves that were constructed to mimic V1154 Cyg as a perfect pulsator modulated only by the light travel time effect caused by low-mass companions. We show that the observed period jitter in V1154 Cyg represents a serious limitation in the search for binary companions. While the Kepler data are accurate enough to allow the detection of planetary bodies in close orbits around a Cepheid, the astrophysical noise can easily hide the signal of the light-time effect.
C1 [Derekas, A.; Szabo, Gy. M.; Szabo, R.; Kiss, L. L.; Szabados, L.] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, H-1121 Budapest, Hungary.
[Derekas, A.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary.
[Derekas, A.; Kiss, L. L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Berdnikov, L.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Berdnikov, L.] Isaac Newton Inst Chile, Moscow Branch, Moscow 119992, Russia.
[Smolec, R.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Chadid, M.] Univ Nice Sophia Antipolis, Observ Cote Azur, UMR 7293, F-06108 Nice 02, France.
[Evans, N. R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Kinemuchi, K.; Seader, S. E.; Smith, J. C.; Tenenbaum, P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada.
[Nemec, J. M.] Int Stat & Res Corp, Brentwood Bay, BC V8M 1R3, Canada.
RP Derekas, A (reprint author), Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos 15-17, H-1121 Budapest, Hungary.
EM derekas@konkoly.hu
RI Smolec, Radoslaw/F-1435-2013; Derekas, Aliz/G-2091-2016;
OI Smolec, Radoslaw/0000-0001-7217-4884; Derekas, Aliz/0000-0002-6526-9444;
Szabo, Robert/0000-0002-3258-1909
FU Hungarian OTKA [K76816, K83790, MB08C 81013]; ESA PECS [C98090];
Hungarian Academy of Sciences; Magyary Zoltan Public Foundation;
Hungarian Eotvos fellowship; NASA's Science Mission Directorate
FX This project has been supported by the Hungarian OTKA Grants K76816,
K83790 and MB08C 81013, ESA PECS C98090 and the 'Lendulet-2009' Young
Researchers Program of the Hungarian Academy of Sciences. AD gratefully
acknowledges financial support from the Magyary Zoltan Public
Foundation. AD was supported by the Hungarian Eotvos fellowship. RS, AD
and GyMSz have been supported by the Janos Bolyai Research Scholarship
of the Hungarian Academy of Sciences. Funding for this Discovery mission
is provided by NASA's Science Mission Directorate. Fruitful discussions
with Zoltan Kollath are gratefully acknowledged.
NR 37
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2012
VL 425
IS 2
BP 1312
EP 1319
DI 10.1111/j.1365-2966.2012.21538.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 993VQ
UT WOS:000307888300038
ER
PT J
AU Ivison, RJ
Smail, I
Amblard, A
Arumugam, V
De Breuck, C
Emonts, BHC
Feain, I
Greve, TR
Haas, M
Ibar, E
Jarvis, MJ
Kovacs, A
Lehnert, MD
Nesvadba, NPH
Rottgering, HJA
Seymour, N
Wylezalek, D
AF Ivison, R. J.
Smail, Ian
Amblard, A.
Arumugam, V.
De Breuck, C.
Emonts, B. H. C.
Feain, I.
Greve, T. R.
Haas, M.
Ibar, E.
Jarvis, M. J.
Kovacs, A.
Lehnert, M. D.
Nesvadba, N. P. H.
Rottgering, H. J. A.
Seymour, N.
Wylezalek, D.
TI Gas-rich mergers and feedback are ubiquitous amongst starbursting radio
galaxies, as revealed by the VLA, IRAM PdBI and Herschel
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE galaxies: active; galaxies: high-redshift; galaxies: starburst;
infrared: galaxies; radio lines: galaxies
ID LUMINOUS SUBMILLIMETER GALAXIES; EXCITATION MOLECULAR GAS; FAR-INFRARED
PROPERTIES; LYMAN-BREAK GALAXIES; LARGE-SCALE SHOCK; EQUAL-TO 3.4;
STAR-FORMATION; CO EMISSION; LARGE ARRAY; CONTINUUM OBSERVATIONS
AB We report new, sensitive observations of two z?similar to?33.5 far-infrared-luminous radio galaxies, 6C?1909+72 and B3?J2330+3927, in the 12CO J = 1-0 transition with the Karl Jansky Very Large Array and at 100500?m using Herschel, alongside new and archival 12CO J = 4-3 observations from the Plateau de Bure Interferometer. We introduce a new colourcolour diagnostic plot to constrain the redshifts of several distant, dusty galaxies in our target fields. A bright SMG near 6C?1909+72 likely shares the same node or filament as the signpost active galactic nuclei (AGN), but it is not detected in 12CO despite similar to 20?000?km?s-1 of velocity coverage. Also in the 6C?1909+72 field, a large, red dust feature spanning 500?kpc is aligned with the radio jet. We suggest several processes by which metal-rich material may have been transported, favouring a collimated outflow reminiscent of the jet-oriented metal enrichment seen in local cluster environments. Our interferometric imaging reveals a gas-rich companion to B3?J2330+3927; indeed, all bar one of the eight z ? 2 radio galaxies (or companions) detected in 12CO provide some evidence that starburst activity in radio-loud AGN at high redshift is driven by the interaction of two or more gas-rich systems in which a significant mass of stars has already formed, rather than via steady accretion of cold gas from the cosmic web. We find that the 12CO brightness temperature ratios in radio-loud AGN host galaxies are significantly higher than those seen in similarly intense starbursts where AGN activity is less pronounced. Our most extreme example, where L CO 4-3'/L CO 1-0'>2.7, provides evidence that significant energy is being deposited rapidly into the molecular gas via X-rays and/or mechanical (quasar-mode) feedback from the AGN, leading to a high degree of turbulence globally and a low optical depth in 12CO feedback that may lead to the cessation of star formation on a time-scale commensurate with that of the jet activity, ?10?Myr.
C1 [Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Sci & Technol Facil Council, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Arumugam, V.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Smail, Ian] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[De Breuck, C.; Wylezalek, D.] European So Observ, D-85748 Garching, Germany.
[Emonts, B. H. C.; Feain, I.; Seymour, N.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Haas, M.] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany.
[Jarvis, M. J.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Kovacs, A.] CALTECH, Pasadena, CA 91125 USA.
[Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA.
[Lehnert, M. D.] Univ Paris Diderot, Observ Paris, GEPI, CNRS,UMR 8111, F-92190 Meudon, France.
[Nesvadba, N. P. H.] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France.
[Rottgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Ivison, RJ (reprint author), Royal Observ, UK Astron Technol Ctr, Sci & Technol Facil Council, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
EM rji@roe.ac.uk
RI Smail, Ian/M-5161-2013; amblard, alexandre/L-7694-2014; Kovacs,
Attila/C-1171-2010; Ivison, R./G-4450-2011;
OI Smail, Ian/0000-0003-3037-257X; amblard, alexandre/0000-0002-2212-5395;
Kovacs, Attila/0000-0001-8991-9088; Ivison, R./0000-0001-5118-1313;
Seymour, Nicholas/0000-0003-3506-5536; De Breuck,
Carlos/0000-0002-6637-3315
FU STFC; Australian Research Council; IDA; DARK; INSU/CNRS (France); MPG
(Germany); IGN (Spain)
FX We are grateful to Arjun Dey, Axel Weiss and Padelis Papadopoulos for
sharing their wisdom regarding superthermal Tb ratios and
unpublished optical spectroscopy. We appreciate the remarkable efforts
of the NRAO staff that have significantly upgraded what many of us
already regarded as the finest telescope ever built. In particular, we
thank Frazer Owen and Gustaaf Van Moorsel for their invaluable help with
the data used here. IRS acknowledges support from STFC and through a
Leverhulme Senior Fellowship. NS is the recipient of an Australian
Research Council Future Fellowship. TRG acknowledges support from STFC,
as well as IDA and DARK. This work is based on observations carried out
with the Karl Janksy Very Large Array. The NRAO is a facility of the NSF
operated under cooperative agreement by Associated Universities, Inc. It
is also based on observations carried out with the IRAM Plateau de Bure
Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany)
and IGN (Spain).
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JI Mon. Not. Roy. Astron. Soc.
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PY 2012
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EP 1331
DI 10.1111/j.1365-2966.2012.21544.x
PG 12
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SC Astronomy & Astrophysics
GA 993VQ
UT WOS:000307888300039
ER
PT J
AU Ramsay, G
Cannizzo, JK
Howell, SB
Wood, MA
Still, M
Barclay, T
Smale, A
AF Ramsay, Gavin
Cannizzo, John K.
Howell, Steve B.
Wood, Matt A.
Still, Martin
Barclay, Thomas
Smale, Alan
TI Kepler observations of V447 Lyr: an eclipsing U Gem Cataclysmic Variable
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: dwarf novae; stars: individual: V447
Lyr; novae, cataclysmic variables
ID V344 LYRAE; DWARF NOVA; LIGHT CURVES; DISK RADIUS; GEMINORUM;
SUPERHUMPS; OUTBURST; SCIENCE; PERFORMANCE
AB We present the results of an analysis of Kepler data covering 1.5 yr of the dwarf nova V447 Lyr. We detect eclipses of the accretion disc by the mass donating secondary star every 3.74 h which is the binary orbital period. V447 Lyr is therefore the first dwarf nova in the Kepler field to show eclipses. We also detect five long outbursts and six short outbursts showing V447 Lyr is a U Gem-type dwarf nova. We show that the orbital phase of the mid-eclipse occurs earlier during outbursts compared to quiescence and that the width of the eclipse is greater during outburst. This suggests that the bright spot is more prominent during quiescence and that the disc is larger during outburst than quiescence. This is consistent with an expansion of the outer disc radius due to the presence of high viscosity material associated with the outburst, followed by a contraction in quiescence due to the accretion of low angular momentum material. We note that the long outbursts appear to be triggered by a short outburst, which is also observed in the super-outbursts of SU UMa dwarf novae as observed using Kepler.
C1 [Ramsay, Gavin] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Cannizzo, John K.] CRESST, Greenbelt, MD 20771 USA.
[Cannizzo, John K.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA.
[Cannizzo, John K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Howell, Steve B.; Still, Martin; Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94095 USA.
[Wood, Matt A.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Still, Martin; Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
RP Ramsay, G (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
EM gar@arm.ac.uk
OI Wood, Matthew/0000-0003-0372-9553
FU NASA, Science Mission Directorate; NASA [NAS5-26555]; NASA Office of
Space Science [NAG5-7584]; National Science Foundation [AST 1109332];
Northern Ireland Executive through the Department of Culture Arts and
Leisure
FX Kepler was selected as the 10th mission of the Discovery Program.
Funding for this mission is provided by NASA, Science Mission
Directorate. All of the data presented in this paper were obtained from
the Multimission Archive at the Space Telescope Science Institute
(MAST). STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for
MAST for non-HST data is provided by the NASA Office of Space Science
via grant NAG5-7584 and by other grants and contracts. This material is
based upon work supported by the National Science Foundation under Grant
No. AST 1109332 to the Florida Institute of Technology. Armagh
Observatory is supported by the Northern Ireland Executive through the
Department of Culture Arts and Leisure.
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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 SEP
PY 2012
VL 425
IS 2
BP 1479
EP 1485
DI 10.1111/j.1365-2966.2012.21657.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 993VQ
UT WOS:000307888300053
ER
PT J
AU Ramsay, G
Wheatley, PJ
Rosen, S
Barclay, T
Steeghs, D
AF Ramsay, Gavin
Wheatley, Peter J.
Rosen, Simon
Barclay, Thomas
Steeghs, Danny
TI Suppression of X-rays during an optical outburst of the helium dwarf
nova KL Dra
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; binaries: general; stars: individual: KL
Dra; stars: dwarf novae; novae, cataclysmic variables; X-rays: stars
ID EXTREME-ULTRAVIOLET FLUX; AM CANUM-VENATICORUM; ACCRETION DISK; SU UMA;
INSTABILITY MODEL; CVN BINARIES; V344 LYRAE; SS-CYGNI; KEPLER;
QUIESCENCE
AB KL Dra is a helium-accreting AM CVn binary system with an orbital period close to 25?min. Approximately every 60?d there is a 4-mag optical outburst lasting similar to 10?d. We present the most sensitive X-ray observations made of an AM CVn system during an outburst cycle. A series of eight observations were made using XMMNewton which started shortly after the onset of an optical outburst. We find that X-rays are suppressed during the optical outburst. There is some evidence for a spectral evolution of the X-ray spectrum during the course of the outburst. A periodic modulation is seen in the ultraviolet data at three epochs this is a signature of the binary orbital or the superhump period. The temperature of the X-ray-emitting plasma is cooler compared to dwarf novae, which may suggest that a wind is the origin of a significant fraction of the X-ray flux.
C1 [Ramsay, Gavin] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Wheatley, Peter J.; Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Rosen, Simon] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
RP Ramsay, G (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
EM gar@arm.ac.uk
RI Steeghs, Danny/C-5468-2009;
OI Steeghs, Danny/0000-0003-0771-4746; Barclay, Thomas/0000-0001-7139-2724;
Wheatley, Peter/0000-0003-1452-2240
FU ESA Member States; USA (NASA); UK Science and Technology Facilities
Council
FX This is work based on observations obtained with XMM-Newton, an ESA
science mission with instruments and contributions directly funded by
ESA Member States and the USA (NASA). 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 financial support from the UK Science
and Technology Facilities Council. We thank the referee, Paul Groot, for
comments which helped improve the paper.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2012
VL 425
IS 2
BP 1486
EP 1491
DI 10.1111/j.1365-2966.2012.21660.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 993VQ
UT WOS:000307888300054
ER
PT J
AU Fleming, SW
Ge, J
Barnes, R
Beatty, TG
Crepp, JR
De Lee, N
Esposito, M
Femenia, B
Ferreira, L
Gary, B
Gaudi, BS
Ghezzi, L
Hernandez, JIG
Hebb, L
Jiang, P
Lee, B
Nelson, B
De Mello, GFP
Shappee, BJ
Stassun, K
Thompson, TA
Tofflemire, BM
Wisniewski, JP
Wood-Vasey, WM
Agol, E
Prieto, CA
Bizyaev, D
Brewington, H
Cargile, PA
Coban, L
Costello, KS
da Costa, LN
Good, ML
Hua, N
Kane, SR
Lander, GR
Liu, J
Ma, B
Mahadevan, S
Maia, MAG
Malanushenko, E
Malanushenko, V
Muna, D
Nguyen, DC
Oravetz, D
Paegert, M
Pan, K
Pepper, J
Rebolo, R
Roebuck, EJ
Santiago, BX
Schneider, DP
Shelden, A
Simmons, A
Sivarani, T
Snedden, S
Vincent, CLM
Wan, XK
Wang, J
Weaver, BA
Weaver, GM
Zhao, B
AF Fleming, Scott W.
Ge, Jian
Barnes, Rory
Beatty, Thomas G.
Crepp, Justin R.
De Lee, Nathan
Esposito, Massimiliano
Femenia, Bruno
Ferreira, Leticia
Gary, Bruce
Gaudi, B. Scott
Ghezzi, Luan
Gonzalez Hernandez, Jonay I.
Hebb, Leslie
Jiang, Peng
Lee, Brian
Nelson, Ben
Porto De Mello, Gustavo F.
Shappee, Benjamin J.
Stassun, Keivan
Thompson, Todd A.
Tofflemire, Benjamin M.
Wisniewski, John P.
Wood-Vasey, W. Michael
Agol, Eric
Allende Prieto, Carlos
Bizyaev, Dmitry
Brewington, Howard
Cargile, Phillip A.
Coban, Louis
Costello, Korena S.
da Costa, Luis N.
Good, Melanie L.
Hua, Nelson
Kane, Stephen R.
Lander, Gary R.
Liu, Jian
Ma, Bo
Mahadevan, Suvrath
Maia, Marcio A. G.
Malanushenko, Elena
Malanushenko, Viktor
Muna, Demitri
Nguyen, Duy Cuong
Oravetz, Daniel
Paegert, Martin
Pan, Kaike
Pepper, Joshua
Rebolo, Rafael
Roebuck, Eric J.
Santiago, Basilio X.
Schneider, Donald P.
Shelden, Alaina
Simmons, Audrey
Sivarani, Thirupathi
Snedden, Stephanie
Vincent, Chelsea L. M.
Wan, Xiaoke
Wang, Ji
Weaver, Benjamin A.
Weaver, Gwendolyn M.
Zhao, Bo
TI VERY LOW MASS STELLAR AND SUBSTELLAR COMPANIONS TO SOLAR-LIKE STARS FROM
MARVELS. II. A SHORT-PERIOD COMPANION ORBITING AN F STAR WITH EVIDENCE
OF A STELLAR TERTIARY AND SIGNIFICANT MUTUAL INCLINATION
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: spectroscopic; stars: individual (TYC
2930-00872-1)
ID HOBBY-EBERLY TELESCOPE; EXTERNALLY DISPERSED INTERFEROMETER; CLOSE
BINARY STARS; PRE-MAIN-SEQUENCE; RADIAL-VELOCITY; TIDAL FRICTION; TRIPLE
STARS; EVOLUTIONARY MODELS; EXTRASOLAR PLANETS; STANDARD STARS
AB We report the discovery via radial velocity (RV) measurements of a short-period (P = 2.430420 +/- 0.000006 days) companion to the F-type main-sequence star TYC 2930-00872-1. A long-term trend in the RV data also suggests the presence of a tertiary stellar companion with P > 2000 days. High-resolution spectroscopy of the host star yields T-eff = 6427 +/- 33 K, log g = 4.52 +/- 0.14, and [Fe/H] = -0.04 +/- 0.05. These parameters, combined with the broadband spectral energy distribution (SED) and a parallax, allow us to infer a mass and radius of the host star of M-1 = 1.21 +/- 0.08 M-circle dot and R-1 = 1.09(-0.13)(+0.15) R-circle dot. The minimum mass of the inner companion is below the hydrogen-burning limit; however, the true mass is likely to be substantially higher. We are able to exclude transits of the inner companion with high confidence. Further, the host star spectrum exhibits a clear signature of Ca H and K core emission, indicating stellar activity, but a lack of photometric variability and small v sin I suggest that the primary's spin axis is oriented in a pole-on configuration. The rotational period of the primary estimated through an activity-rotation relation matches the orbital period of the inner companion to within 1.5 sigma, suggesting that the primary and inner companion are tidally locked. If the inner companion's orbital angular momentum vector is aligned with the stellar spin axis as expected through tidal evolution, then it has a stellar mass of similar to 0.3-0.4 M-circle dot. Direct imaging limits the existence of stellar companions to projected separations <30 AU. No set of spectral lines and no significant flux contribution to the SED from either companion are detected, which places individual upper mass limits of M-{2,M-3} less than or similar to 1.0 M-circle dot, provided they are not stellar remnants. If the tertiary is not a stellar remnant, then it likely has a mass of similar to 0.5-0.6M(circle dot), and its orbit is likely significantly inclined from that of the secondary, suggesting that the Kozai-Lidov mechanism may have driven the dynamical evolution of this system.
C1 [Fleming, Scott W.; Ge, Jian; De Lee, Nathan; Jiang, Peng; Lee, Brian; Nelson, Ben; Liu, Jian; Ma, Bo; Nguyen, Duy Cuong; Wan, Xiaoke; Wang, Ji; Zhao, Bo] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32610 USA.
[Fleming, Scott W.; Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Fleming, Scott W.; Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Barnes, Rory; Tofflemire, Benjamin M.; Wisniewski, John P.; Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Beatty, Thomas G.; Gaudi, B. Scott; Shappee, Benjamin J.; Thompson, Todd A.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Crepp, Justin R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[De Lee, Nathan; Gary, Bruce; Hebb, Leslie; Stassun, Keivan; Cargile, Phillip A.; Paegert, Martin; Pepper, Joshua] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Esposito, Massimiliano; Femenia, Bruno; Gonzalez Hernandez, Jonay I.; Allende Prieto, Carlos; Rebolo, Rafael] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Esposito, Massimiliano; Femenia, Bruno; Gonzalez Hernandez, Jonay I.; Allende Prieto, Carlos; Rebolo, Rafael] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Ferreira, Leticia; Porto De Mello, Gustavo F.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, RJ, Brazil.
[Ferreira, Leticia; Ghezzi, Luan; Porto De Mello, Gustavo F.; da Costa, Luis N.; Maia, Marcio A. G.; Santiago, Basilio X.] LIneA, Lab Interinst Astron, Rio De Janeiro, RJ, Brazil.
[Ghezzi, Luan; da Costa, Luis N.; Maia, Marcio A. G.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[Stassun, Keivan] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Tofflemire, Benjamin M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Wood-Vasey, W. Michael; Coban, Louis; Costello, Korena S.; Good, Melanie L.; Hua, Nelson; Lander, Gary R.; Roebuck, Eric J.; Vincent, Chelsea L. M.; Weaver, Gwendolyn M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Bizyaev, Dmitry; Brewington, Howard; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Shelden, Alaina; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA.
[Kane, Stephen R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Muna, Demitri; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Nguyen, Duy Cuong] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Rebolo, Rafael] CSIC, E-28006 San Cristobal la Laguna, Spain.
[Santiago, Basilio X.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil.
[Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
RP Fleming, SW (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32610 USA.
EM scfleming@psu.edu
RI Gaudi, Bernard/I-7732-2012; Kane, Stephen/B-4798-2013; Agol,
Eric/B-8775-2013; Gonzalez Hernandez, Jonay I./L-3556-2014;
OI Agol, Eric/0000-0002-0802-9145; Gonzalez Hernandez, Jonay
I./0000-0002-0264-7356; Fleming, Scott/0000-0003-0556-027X; Nelson,
Benjamin/0000-0003-3010-2334; Pepper, Joshua/0000-0002-3827-8417
FU Vanderbilt Initiative in Data-Intensive Astrophysics (VIDA) from
Vanderbilt University; NSF [AST-0349075, AST-0645416, AST 08-02230,
AST-1056524, AST-0908816, AST-0705139]; PAPDRJ CAPES/FAPERJ; CAPES; ESO;
CNPq [476909/2006-6, 474972/2009-7]; FAPERJ [APQ1/26/170.687/2004];
Pennsylvania Space Grant Consortium; Alfred P. Sloan Foundation;
National Science Foundation; Center for Exoplanets and Habitable Worlds;
Pennsylvania State University; Eberly College of Science; National
Aeronautics and Space Administration; W. M. Keck Foundation; SDSS-III
consortium; NASA [NNX07AP14G]; University of Florida; Instituto
Nazionale di Astrofisica (INAF), in the Spanish Observatorio del Roque
de los Muchachos of the Instituto de Astrofisica de Canarias (IAC); U.S.
Department of Energy Office of Science; University of Arizona; Brazilian
Participation Group; Brookhaven National Laboratory; University of
Cambridge; Carnegie Mellon University; French Participation Group;
German Participation Group; Harvard University; Instituto de Astrofisica
de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max-Planck-Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; University of Portsmouth; Princeton University; Spanish
Participation Group; University of Tokyo; University of Utah; Vanderbilt
University; University of Virginia; University of Washington; Yale
University
FX K.S., L. H., and J.P. acknowledge funding support from the Vanderbilt
Initiative in Data-Intensive Astrophysics (VIDA) from Vanderbilt
University and from NSF Career Award AST-0349075. E. A. thanks the NSF
for Career Grant AST-0645416. J.W. acknowledges support from NSF
Astronomy and Astrophysics Postdoctoral Fellowship AST 08-02230. L. G.
acknowledges financial support provided by the PAPDRJ CAPES/FAPERJ
Fellowship. L.D.-F. acknowledges financial support provided by CAPES and
ESO student fellowship. G.F.P.d.M. acknowledges financial support from
CNPq grant Nos. 476909/2006-6 and 474972/2009-7, plus a FAPERJ grant No.
APQ1/26/170.687/2004. C. V. and G. W. acknowledge support from the
Pennsylvania Space Grant Consortium. Operation of Allegheny Observatory
is supported in part by the Theiss Memorial Endowment. Work by B. S. G.
and T. B. was partially supported by NSF Career Grant AST-1056524. We
thank J. Fregeau for making the code FEWBODY publicly available. This
work is supported in part by an Alfred P. Sloan Foundation Fellowship
and NSF Grant AST-0908816. B. S. was supported by a Graduate Research
Fellowship from the National Science Foundation.; This work was
partially supported by funding from the Center for Exoplanets and
Habitable Worlds. The Center for Exoplanets and Habitable Worlds is
supported by the Pennsylvania State University, the Eberly College of
Science, and the Pennsylvania Space Grant Consortium. This research has
made use of the SIMBAD database, operated at CDS, Strasbourg, France.
This publication makes use of data products from the Two Micron All Sky
Survey, which is a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. This publication makes use of data
products from the Wide-field Infrared Survey Explorer, which is a joint
project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration.; Funding for the MARVELS
multi-object Doppler instrument was provided by the W. M. Keck
Foundation and NSF with grant AST-0705139. The MARVELS survey was
partially funded by the SDSS-III consortium, NSF Grant AST-0705139, NASA
with grant NNX07AP14G and the University of Florida. This work has made
use of observations taken with the Telescopio Nationale Galileo (TNG)
operated on the island of La Palma by the Fundation Galileo Galilei,
funded by the Instituto Nazionale di Astrofisica (INAF), in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias (IAC).; This work was based on observations with the SDSS
2.5 m telescope. 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/Notre Dame/JINA Participation Group, Johns Hopkins
University, Lawrence Berkeley National Laboratory, Max Planck Institute
for Astrophysics, Max-Planck-Institute for Extraterrestrial Physics, New
Mexico State University, New York University, Ohio State University,
Pennsylvania State University, University of Portsmouth, Princeton
University, the Spanish Participation Group, University of Tokyo,
University of Utah, Vanderbilt University, University of Virginia,
University of Washington, and Yale University.
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JI Astron. J.
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SC Astronomy & Astrophysics
GA 995JF
UT WOS:000308003600002
ER
PT J
AU Gomez, PL
Valkonen, LE
Romer, AK
Lloyd-Davies, E
Verdugo, T
Cantalupo, CM
Daub, MD
Goldstein, JH
Kuo, CL
Lange, AE
Lueker, M
Holzapfel, WL
Peterson, JB
Ruhl, J
Runyan, MC
Reichardt, CL
Sabirli, K
AF Gomez, P. L.
Valkonen, L. E.
Romer, A. K.
Lloyd-Davies, E.
Verdugo, T.
Cantalupo, C. M.
Daub, M. D.
Goldstein, J. H.
Kuo, C. L.
Lange, A. E.
Lueker, M.
Holzapfel, W. L.
Peterson, J. B.
Ruhl, J.
Runyan, M. C.
Reichardt, C. L.
Sabirli, K.
TI OPTICAL AND X-RAY OBSERVATIONS OF THE MERGING CLUSTER AS1063
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general
ID RELAXED GALAXY CLUSTERS; RICH CLUSTERS; INTRACLUSTER MEDIUM; HOT PLASMA;
ABELL 3266; SUBSTRUCTURE; CATALOG; MASS; THERMODYNAMICS; EVOLUTION
AB We present the first in-depth analysis of the massive cluster AS1063. This is one of the hottest X-ray clusters discovered to date and is undergoing a major merging event. The average temperature of the hot intracluster medium has been measured, using Chandra/ACIS-I, and found to be >11.5 keV. Optical spectroscopy, from GMOS-S, has provided a mean redshift of 0.3461 and a large velocity dispersion of 1840(-150)(+230) km s(.)(-1) Both the large velocity dispersion and high X-ray temperature suggest a very massive cluster (M-200 > 2.5 x 10(15) M-circle dot) and/or a merger system. The merger model is supported by a small offset between the galaxy density and the peak of the X-ray emission, the presence of offset and twisted X-ray isophotes, and a non-Gaussian galaxy velocity distribution. We also report that the velocity distribution is better represented by the velocity dispersion produced during a merger than by the velocity distribution of a relaxed cluster. Moreover, we find that two non-concentric beta models are a better description for the distribution of the cluster gas than a single beta model. Therefore, we propose that a recent merger event close to the plane of the sky is responsible for the observed properties of the cluster. In addition, optical imaging, from SuSI2 on the New Technology Telescope and GMOS-S at Gemini, has also uncovered the presence of several gravitational arcs that have been used to further constrain the mass and dynamics of the cluster.
C1 [Gomez, P. L.] AURA, So Operat Ctr, Gemini Observ, La Serena, Chile.
[Valkonen, L. E.; Romer, A. K.; Lloyd-Davies, E.; Ruhl, J.; Sabirli, K.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Verdugo, T.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile.
[Cantalupo, C. M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Daub, M. D.; Lueker, M.; Holzapfel, W. L.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Goldstein, J. H.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Goldstein, J. H.] Arrete Associates, Arlington, VA 22202 USA.
[Kuo, C. L.; Lange, A. E.; Runyan, M. C.] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA.
[Kuo, C. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Kuo, C. L.] Stanford Univ, KIPAC, Stanford, CA 94305 USA.
[Lange, A. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Peterson, J. B.; Sabirli, K.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
RP Gomez, PL (reprint author), AURA, So Operat Ctr, Gemini Observ, Casilla 603, La Serena, Chile.
RI Holzapfel, William/I-4836-2015;
OI Reichardt, Christian/0000-0003-2226-9169; Verdugo,
Tomas/0000-0003-4062-6123
FU NASA [NAG5-7926, NAG5-12999, NAG5-20453, GO4-5141X]; European Commission
[EIF-OIF-IIF-IRG-ERG, 513676]; AAS; STFC (the UK Science and Technology
Facilities Council); Osk. Huttunen Foundation; Magnus Ehrnrooth
Foundation; University of Sussex Physics and Astronomy Department for a
Graduate Teaching Assistantship; National Aeronautics Space
Administration [NAS8-03060]; ESO telescopes at La Silla [70.A-0074]
FX This research was possible with financial support from: (1) NASA (via
the XMM and Chandra Guest Observer programs and the Long Term Space
Astrophysics program, grant Nos. NAG5-7926, NAG5-12999, NAG5-20453,
GO4-5141X); (2) the European Commission (via a Marie Curie Reintegration
Grant, grant number EIF-OIF-IIF-IRG-ERG; Project 513676); (3) AAS (via
international travel grants for 2003 and 2004 and a small research
grant); (4) STFC (the UK Science and Technology Facilities Council) (K.
R., P. G.); (5) the Osk. Huttunen Foundation for a PhD studentship (L.
V.); (6) the Magnus Ehrnrooth Foundation for a travel grant (L. V.); and
(7) the University of Sussex Physics and Astronomy Department for a
Graduate Teaching Assistantship (L. V.). In addition P. L. G. thanks the
kindness of the Sussex Astronomy Centre during month long visits in 2006
and 2007. P. L. G. also thanks the European Southern Observatory (ESO)
for two short stays at their Headquarters in Santiago where a large
fraction of the final version of this paper was written. Finally, we
thank the referees for helping us write a more concise, accurate, and
hopefully interesting paper.; This work is based on observations
obtained from (1) 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), Ministrio da Cincia e Tecnologia (Brazil), and SECYT
(Argentina); (2) the Chandra X-Ray Observatory (Chandra) is operated by
the Smithsonian Astrophysical Observatory for and on behalf of the
National Aeronautics Space Administration under contract NAS8-03060; and
(3) the ESO telescopes at La Silla under program 70.A-0074.
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SN 0004-6256
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JI Astron. J.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 995JF
UT WOS:000308003600009
ER
PT J
AU Nugent, CR
Mainzer, A
Masiero, J
Grav, T
Bauer, J
AF Nugent, C. R.
Mainzer, A.
Masiero, J.
Grav, T.
Bauer, J.
TI THE YARKOVSKY DRIFT'S INFLUENCE ON NEAs: TRENDS AND PREDICTIONS WITH
NEOWISE MEASUREMENTS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; minor planets, asteroids: general; minor planets, asteroids:
individual (2010 JG87, 2006 HY51, (137924) 2000 BD19, 2010 HX107, 2002
LT24, (153201) 2000 WO107, 2010 EX11, 2008 EY5, 2006 NL, 2006 MD12, 2010
GQ75); radiation mechanisms: thermal
ID THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; EARTH ASTEROIDS;
SEMIMAJOR AXIS
AB We used WISE-derived geometric albedos (p(V)) and diameters, as well as geometric albedos and diameters from the literature, to produce more accurate diurnal Yarkovsky drift predictions for 540 near-Earth asteroids (NEAs) out of the current sample of similar to 8800 known objects. As 10 of the 12 objects with the fastest predicted rates have observed arcs of less than a decade, we list upcoming apparitions of these NEAs to facilitate observations.
C1 [Nugent, C. R.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Mainzer, A.; Masiero, J.; Bauer, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ USA.
RP Nugent, CR (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This publication also makes use of data products from
NEOWISE, which is a project of the Jet Propulsion Laboratory/California
Institute of Technology, funded by the Planetary Science Division of the
National Aeronautics and Space Administration. We gratefully acknowledge
the extraordinary services specific to NEOWISE contributed by the
International Astronomical Unions Minor Planet Center, operated by the
Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for
Astronomical Telegrams, operated by Harvard University. We also thank
the worldwide community of dedicated amateur and professional
astronomers devoted to minor planet follow-up observations. 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2012
VL 144
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DI 10.1088/0004-6256/144/3/75
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 995JF
UT WOS:000308003600005
ER
PT J
AU Bansal, NP
Wise, B
AF Bansal, Narottam P.
Wise, Brent
TI Sol-gel synthesis of La0.6Sr0.4CoO3-x and Sm0.5Sr0.5CoO3-x cathode
nanopowders for solid oxide fuel cells
SO CERAMICS INTERNATIONAL
LA English
DT Article
DE Perovskites; Solid oxide fuel cell; Cathodes; Nanopowders
ID PEROVSKITES
AB Nano-powders of La0.6Sr0.4CoO3-x (LSC) and Sm0.5Sr0.5CoO3-x (SSC) compositions, which are being investigated as cathode materials for intermediate temperature solid oxide fuel cells (IT-SOFCs) with La(Sr)Ga(Mg)O3-x (LSGM) as the electrolyte, were synthesized by low-temperature sol-gel method using metal nitrates and citric acid. Thermal decomposition of the citrate gels was followed by simultaneous DSC/TGA methods. Development of phases in the gels, on heat treatments at various temperatures, was monitored by X-ray diffraction. Sol-gel powders calcined at 550-1000 degrees C consisted of a number of phases. Single perovskite phase La0.6Sr0.4CoO3-x or Sm0.5Sr0.5CoO3-x powders were obtained at 1200 degrees C and 1300 degrees C, respectively. Morphological analysis of the powders calcined at various temperatures was done by scanning electron microscopy. The average crystallite size of the powders was,similar to 15 nm after 700 degrees C calcinations and slowly increased to 70-100 nm after heat treatments at 1300-1400 degrees C. Published by Elsevier Ltd and Techna Group S.r.l.
C1 [Bansal, Narottam P.; Wise, Brent] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Bansal, NP (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Narottam.P.Bansal@nasa.gov
FU NASA's Subsonic Fixed Wing Project of the Fundamental Aeronautics
Program
FX Thanks are due to John Setlock for DSC-TGA and to Ralph Garlick for
X-ray diffraction analysis. This work was supported by NASA's Subsonic
Fixed Wing Project of the Fundamental Aeronautics Program. Brent Wise
was a co-op student from Case Western Reserve University at NASA Glenn
Research Center during the time this work was carried out.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0272-8842
J9 CERAM INT
JI Ceram. Int.
PD SEP
PY 2012
VL 38
IS 7
BP 5535
EP 5541
DI 10.1016/j.ceramint.2012.03.069
PG 7
WC Materials Science, Ceramics
SC Materials Science
GA 982FD
UT WOS:000307027300029
ER
PT J
AU Roeder, AHK
Cunha, A
Burl, MC
Meyerowitz, EM
AF Roeder, Adrienne H. K.
Cunha, Alexandre
Burl, Michael C.
Meyerowitz, Elliot M.
TI A computational image analysis glossary for biologists
SO DEVELOPMENT
LA English
DT Article
DE Segmentation; Filtering; Registration; Volume rendering; Morphological
image processing; Image analysis
AB Recent advances in biological imaging have resulted in an explosion in the quality and quantity of images obtained in a digital format. Developmental biologists are increasingly acquiring beautiful and complex images, thus creating vast image datasets. In the past, patterns in image data have been detected by the human eye. Larger datasets, however, necessitate high-throughput objective analysis tools to computationally extract quantitative information from the images. These tools have been developed in collaborations between biologists, computer scientists, mathematicians and physicists. In this Primer we present a glossary of image analysis terms to aid biologists and briefly discuss the importance of robust image analysis in developmental studies.
C1 [Roeder, Adrienne H. K.; Meyerowitz, Elliot M.] CALTECH, Div Biol, Pasadena, CA 91125 USA.
[Roeder, Adrienne H. K.; Cunha, Alexandre] CALTECH, Ctr Integrat Study Cell Regulat, Pasadena, CA 91125 USA.
[Cunha, Alexandre] CALTECH, Ctr Adv Comp Res, Pasadena, CA 91125 USA.
[Burl, Michael C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Meyerowitz, Elliot M.] Univ Cambridge, Sainsbury Lab, Cambridge CB2 1LR, England.
RP Roeder, AHK (reprint author), Cornell Univ, Dept Plant Biol, Ithaca, NY 14853 USA.
EM aroeder@cornell.edu
OI Roeder, Adrienne/0000-0001-6685-2984
FU Department of Energy Office of Basic Energy Sciences, Division of
Chemical Sciences, Geosciences and Biosciences, Office of Basic Energy
Sciences of the U.S. Department of Energy; Gordon and Betty Moore
Foundation Cell Center at Caltech; Helen Hay Whitney Foundation
FX We acknowledge the Department of Energy Office of Basic Energy Sciences,
Division of Chemical Sciences, Geosciences and Biosciences, Office of
Basic Energy Sciences of the U.S. Department of Energy (E. M. M.) for
funding the experimental research that has provided the images of sepals
that are used in the examples given, the Gordon and Betty Moore
Foundation Cell Center at Caltech (A. H. K. R. and A. C.) for funding
the computational image processing of those images, and a Helen Hay
Whitney Foundation postdoctoral fellowship to A.H.K.R.
NR 4
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PU COMPANY OF BIOLOGISTS LTD
PI CAMBRIDGE
PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL,
CAMBS, ENGLAND
SN 0950-1991
J9 DEVELOPMENT
JI Development
PD SEP 1
PY 2012
VL 139
IS 17
BP 3071
EP 3080
DI 10.1242/dev.076414
PG 10
WC Developmental Biology
SC Developmental Biology
GA 994IX
UT WOS:000307925200002
PM 22872081
ER
PT J
AU Chan, YK
Lacap, DC
Lau, MCY
Ha, KY
Warren-Rhodes, KA
Cockell, CS
Cowan, DA
McKay, CP
Pointing, SB
AF Chan, Yuki
Lacap, Donnabella C.
Lau, Maggie C. Y.
Ha, Kong Ying
Warren-Rhodes, Kimberley A.
Cockell, Charles S.
Cowan, Donald A.
McKay, Christopher P.
Pointing, Stephen B.
TI Hypolithic microbial communities: between a rock and a hard place
SO ENVIRONMENTAL MICROBIOLOGY
LA English
DT Review
ID ANTARCTIC DRY VALLEY; RADIATION-RESISTANCE; ENVIRONMENTAL GRADIENTS;
POLAR DESERT; CHINA HOT; CYANOBACTERIAL; DIVERSITY; ECOLOGY; ALGAE;
PHOTOSYNTHESIS
AB Drylands are the largest terrestrial biome on Earth and a ubiquitous feature is desert pavement terrain, comprising rocks embedded in the mineral soil surface. Quartz and other translucent rocks are common and microbial communities termed hypoliths develop as biofilms on their ventral surfaces. In extreme deserts these represent major concentrations of biomass, and are emerging as key to geobiological processes and soil stabilization. These highly specialized communities are dominated by cyanobacteria that support diverse heterotrophic assemblages. Here we identify global-scale trends in the ecology of hypoliths that are strongly related to climate, particularly with regard to shifts in cyanobacterial assemblages. A synthesis of available data revealed a linear trend for colonization with regard to climate, and we suggest potential application for hypoliths as biomarkers of aridity on a landscape scale. The potential to exploit the soil-stabilizing properties of hypolithic colonization in environmental engineering on dryland soils is also discussed.
C1 [Chan, Yuki; Lacap, Donnabella C.; Ha, Kong Ying; Pointing, Stephen B.] Univ Hong Kong, Sch Biol Sci, Hong Kong, Hong Kong, Peoples R China.
[Lau, Maggie C. Y.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA.
[Warren-Rhodes, Kimberley A.; McKay, Christopher P.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Cockell, Charles S.] Univ Edinburgh, Sch Phys & Astron, Edinburgh EH9 3JZ, Midlothian, Scotland.
[Cowan, Donald A.] Univ Western Cape, Inst Microbial Biotechnol & Metagenom, ZA-7535 Cape Town, South Africa.
[Pointing, Stephen B.] Auckland Univ Technol, Sch Appl Sci, Auckland 1142, New Zealand.
RP Pointing, SB (reprint author), Univ Hong Kong, Sch Biol Sci, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
EM steve.pointing@aut.ac.nz
RI Cowan, Don/E-3991-2012;
OI Cowan, Don/0000-0001-8059-861X; Chan, Yuki/0000-0002-9570-5462
FU NASA Astrobiology Science and Technology for Exploring Planets (ASTEP)
Programme; Hong Kong Research Grants Council [HKU 7733/08M, HKU
7763/10]; South African National Research Foundation SANAP programme
FX This review emerged from discussion at NASA's Spaceward Bound Expedition
to the Namib Desert in 2010. The research was supported by the NASA
Astrobiology Science and Technology for Exploring Planets (ASTEP)
Programme, the Hong Kong Research Grants Council (Grant numbers HKU
7733/08M HKU 7763/10) and the South African National Research Foundation
SANAP programme.
NR 53
TC 35
Z9 37
U1 4
U2 42
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1462-2912
J9 ENVIRON MICROBIOL
JI Environ. Microbiol.
PD SEP
PY 2012
VL 14
IS 9
SI SI
BP 2272
EP 2282
DI 10.1111/j.1462-2920.2012.02821.x
PG 11
WC Microbiology
SC Microbiology
GA 999HN
UT WOS:000308300600003
PM 22779750
ER
PT J
AU Langlois, TJ
Radford, BT
Van Niel, KP
Meeuwig, JJ
Pearce, AF
Rousseaux, CSG
Kendrick, GA
Harvey, ES
AF Langlois, Timothy J.
Radford, Ben T.
Van Niel, Kimberley P.
Meeuwig, Jessica J.
Pearce, Alan F.
Rousseaux, Cecile S. G.
Kendrick, Gary A.
Harvey, Euan S.
TI Consistent abundance distributions of marine fishes in an old,
climatically buffered, infertile seascape
SO GLOBAL ECOLOGY AND BIOGEOGRAPHY
LA English
DT Article
DE Abundance distribution; abundant-centre; Australia; demersal fish;
Indian Ocean; latitude; ocean solutions; species turnover
ID CLIMATE-CHANGE; CONTINENTAL-SLOPE; CENTER HYPOTHESIS; SPECIES RICHNESS;
VIDEO STATIONS; CURRENT SYSTEM; PACIFIC COAST; REEF FISHES;
BIODIVERSITY; SOUTHERN
AB Aim Macroecological theory predicts that along direct physiological gradients there will be unimodal abundance distributions of species and consistent rates of assemblage turnover. However, the majority of marine studies that have investigated the realized distribution of species along latitudinal or temperature gradients have generally found unimodal distributions to be rare. We assess fish distributions along a temperature gradient in a stable oligotrophic seascape and suggest that unimodal distributions will be more common. Location Nearshore demersal fish habitat extending 1500 km along the coast of south-western Australia. Methods The relative abundances of demersal fish species were sampled off the coast of south-western Australia along a temperature gradient. The confounding influence of other environmental variables was tested, and the assemblage was found to be highly correlated with temperature. For the 20 most abundant species, quantile regression spline models were used to construct a model within which 95% of their abundance was expected to fall. We compared the results from this study with the proportion of unimodal species abundance distributions observed in other studies. Results Of the 20 most abundant species, 19 displayed patterns that indicated temperature was an important factor influencing their range and relative abundance; with 15 species exhibiting unimodal abundance distributions, four having ramped distribution to one end of the sampled range and one showing no consistent pattern. Main conclusions The high diversity and percentage of endemic species in terrestrial and marine habitats of south-western Australia is likely to be due to the stable geological and oceanographic history of the region. In comparison, studies of abundance distribution in other marine systems have been conducted in relatively heterogeneous and productive environments. The old, climatically buffered, oligotrophic seascape of south-western Australia has provided a simple system in which the consistent influence of physiological gradients on the abundance distribution of fish species can be observed.
C1 [Langlois, Timothy J.] Univ Western Australia, UWA Oceans Inst M470, Sch Plant Biol, Crawley, WA 6009, Australia.
[Langlois, Timothy J.; Van Niel, Kimberley P.; Meeuwig, Jessica J.; Rousseaux, Cecile S. G.; Kendrick, Gary A.; Harvey, Euan S.] Univ Western Australia, UWA Oceans Inst, Crawley, WA 6009, Australia.
[Radford, Ben T.; Van Niel, Kimberley P.] Univ Western Australia, Sch Earth & Environm, Crawley, WA 6009, Australia.
[Radford, Ben T.] Univ Western Australia, Australian Inst Marine Sci, Crawley, WA 6009, Australia.
[Rousseaux, Cecile S. G.] Univ Western Australia, Sch Environm Syst Engn, Crawley, WA 6009, Australia.
[Meeuwig, Jessica J.] Univ Western Australia, Ctr Marine Futures, Crawley, WA 6009, Australia.
[Meeuwig, Jessica J.] Univ Western Australia, Sch Anim Biol, Crawley, WA 6009, Australia.
[Pearce, Alan F.] Curtin Univ Technol, Dept Imaging & Appl Phys, Bentley, WA 6102, Australia.
[Rousseaux, Cecile S. G.] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Langlois, TJ (reprint author), Univ Western Australia, UWA Oceans Inst M470, Sch Plant Biol, 35 Stirling Highway, Crawley, WA 6009, Australia.
EM timothy.langlois@uwa.edu.au
RI Rousseaux, Cecile/E-8811-2012; Kendrick, Gary/B-3460-2011; Harvey,
Euan/B-2896-2011; Langlois, Tim/H-5241-2014
OI Rousseaux, Cecile/0000-0002-3022-2988; Kendrick,
Gary/0000-0002-0276-6064; Harvey, Euan/0000-0002-9069-4581;
NR 54
TC 23
Z9 23
U1 0
U2 29
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1466-822X
J9 GLOBAL ECOL BIOGEOGR
JI Glob. Ecol. Biogeogr.
PD SEP
PY 2012
VL 21
IS 9
BP 886
EP 897
DI 10.1111/j.1466-8238.2011.00734.x
PG 12
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 993YS
UT WOS:000307897200002
ER
PT J
AU Miller, SG
Roberts, GD
Bail, JL
Kohlman, LW
Binienda, WK
AF Miller, Sandi G.
Roberts, Gary D.
Bail, Justin L.
Kohlman, Lee W.
Binienda, Wieslaw K.
TI Effects of hygrothermal cycling on the chemical, thermal, and mechanical
properties of 862/W epoxy resin
SO HIGH PERFORMANCE POLYMERS
LA English
DT Article
DE epoxy resin; hygrothermal aging; differential scanning calorimetry;
physical aging
ID AMINE NETWORKS; COMPOSITES; DEGRADATION; DIFFUSION; OXIDATION; MOISTURE;
MATRIX
AB The hygrothermal aging characteristics of an epoxy resin were characterized over a one-year period, which included 908 temperature and humidity cycles. The epoxy resin quickly displayed evidence of aging through color change and increased brittleness. The influence of aging on the material's glass transition temperature (T-g) was evaluated by Differential Scanning Calorimetry and Dynamic Mechanical Analysis. The T-g remained relatively constant throughout the year-long cyclic aging profile. Chemical composition was monitored by Fourier Transform Infrared spectroscopy, where evidence of chemical aging and advancement of cure was noted. The tensile strength of the resin was tested as it aged and this property was severely affected by the aging process in the form of reduced ductility and embrittlement. Detailed chemical evaluation suggests many aging mechanisms are taking place during exposure to hygrothermal conditions.
C1 [Miller, Sandi G.; Roberts, Gary D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Kohlman, Lee W.; Binienda, Wieslaw K.] Univ Akron, Akron, OH 44325 USA.
RP Miller, SG (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Sandi.G.Miller@nasa.gov
FU NASA Fundamental Aeronautics/ Aviation Safety Program
FX This work was funded through the NASA Fundamental Aeronautics/ Aviation
Safety Program.
NR 18
TC 10
Z9 10
U1 0
U2 17
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0954-0083
J9 HIGH PERFORM POLYM
JI High Perform. Polym.
PD SEP
PY 2012
VL 24
IS 6
BP 470
EP 477
DI 10.1177/0954008312443273
PG 8
WC Polymer Science
SC Polymer Science
GA 993EI
UT WOS:000307838200003
ER
PT J
AU Crichton, DJ
Mattmann, CA
Cinquini, L
Braverman, A
Waliser, D
Gunson, M
Hart, AF
Goodale, CE
Lean, P
Kim, J
AF Crichton, Daniel J.
Mattmann, Chris A.
Cinquini, Luca
Braverman, Amy
Waliser, Duane
Gunson, Michael
Hart, Andrew F.
Goodale, Cameron E.
Lean, Peter
Kim, Jinwon
TI Sharing Satellite Observations with the Climate-Modeling Community:
Software and Architecture
SO IEEE SOFTWARE
LA English
DT Article
ID ACCESS; SYSTEM
C1 [Crichton, Daniel J.; Mattmann, Chris A.; Cinquini, Luca; Braverman, Amy; Waliser, Duane; Gunson, Michael; Hart, Andrew F.; Goodale, Cameron E.] NASA, Jet Prop Lab, Washington, DC 20546 USA.
[Gunson, Michael] NASA, Orbiting Carbon Observ Oco 2, Washington, DC USA.
[Lean, Peter] Univ Reading, Reading RG6 2AH, Berks, England.
[Kim, Jinwon] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Crichton, DJ (reprint author), NASA, Jet Prop Lab, Washington, DC 20546 USA.
EM crichton@jpl.nasa.gov; mattmann@jpl.nasa.gov;
luca.cinquini@jpl.nasa.gov; ajb@jpl.nasa.gov; waliser@jpl.nasa.gov;
mgunson@jpl.nasa.gov; andrew.f.hart@jpl.nasa.gov;
cameron.e.goodale@jpl.nasa.gov; p.w.lean@reading.ac.uk;
jkim@atmos.ucla.edu
NR 11
TC 3
Z9 3
U1 1
U2 4
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0740-7459
J9 IEEE SOFTWARE
JI IEEE Softw.
PD SEP-OCT
PY 2012
VL 29
IS 5
BP 73
EP 81
PG 9
WC Computer Science, Software Engineering
SC Computer Science
GA 991HD
UT WOS:000307691200019
ER
PT J
AU Smith, SM
Heer, MA
Shackelford, LC
Sibonga, JD
Ploutz-Snyder, L
Zwart, SR
AF Smith, Scott M.
Heer, Martina A.
Shackelford, Linda C.
Sibonga, Jean D.
Ploutz-Snyder, Lori
Zwart, Sara R.
TI Benefits for bone from resistance exercise and nutrition in
long-duration spaceflight: Evidence from biochemistry and densitometry
SO JOURNAL OF BONE AND MINERAL RESEARCH
LA English
DT Article
DE VITAMIN D; BONE LOSS; BONE TURNOVER MARKERS; SPACE FLIGHT;
WEIGHTLESSNESS
ID INTERNATIONAL-SPACE-STATION; BED REST; RESISTIVE EXERCISE;
ENERGY-EXPENDITURE; CALCIUM-METABOLISM; PROTEIN-METABOLISM; FLIGHT;
ASTRONAUTS; HUMANS; SUPPLEMENTATION
AB Exercise has shown little success in mitigating bone loss from long-duration spaceflight. The first crews of the International Space Station (ISS) used the interim resistive exercise device (iRED), which allowed loads of up to 297 lbf (or 1337 N) but provided little protection of bone or no greater protection than aerobic exercise. In 2008, the Advanced Resistive Exercise Device (ARED), which allowed absolute loads of up to 600 lbf (1675 N), was launched to the ISS. We report dietary intake, bone densitometry, and biochemical markers in 13 crewmembers on ISS missions from 2006 to 2009. Of these 13, 8 had access to the iRED and 5 had access to the ARED. In both groups, bone-specific alkaline phosphatase tended to increase during flight toward the end of the mission (p?=?0.06) and increased 30 days after landing (p? 9.5 drawn from the Great Observatories Origins Deep Survey (GOODS) Near Infrared Camera and Multi-Object Spectrometer (NICMOS) Survey (GNS), the deepest H-band Hubble Space Telescope survey of its type prior to the installation of Wide Field Camera 3 (WFC3). We use far-IR and submm data from the Photoconductor Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) instruments on-board Herschel, taken from the PACS Evolutionary Probe (PEP) and Herschel Multi-Tiered Extragalactic Survey (HerMES) key projects, respectively. We find a total of 22 GNS galaxies, with median log?(M*/M?) = 10.8 and z = 2.0, associated with 250?mu m sources detected with signal-to-noise ratio (SNR) > 3. We derive mean total IR luminosity log?LIR(L?) = 12.36 +/- 0.05 and corresponding star formation rate (SFR)IR + UV = (280 +/- 40)?M??yr-1 for these objects, and find them to have mean dust temperature Tdust similar to 35?K. We find that the SFR derived from the far-IR photometry combined with ultraviolet (UV)-based estimates of unobscured SFR for these galaxies is on average more than a factor of 2 higher than the SFR derived from extinction-corrected UV emission alone, although we note that the IR-based estimate is subject to substantial Malmquist bias. To mitigate the effect of this bias and extend our study to fainter fluxes, we perform a stacking analysis to measure the mean SFR in bins of stellar mass. We obtain detections at the 24s level at SPIRE wavelengths for samples with log?(M*/M?) > 10. In contrast to the Herschel detected GNS galaxies, we find that estimates of SFRIR + UV for the stacked samples are comparable to those derived from extinction-corrected UV emission, although the uncertainties are large. We find evidence for an increasing fraction of dust obscured star formation with stellar mass, finding SFR IR / SFR UV ?M*0.7 +/- 0.2, which is likely a consequence of the massmetallicity relation.
C1 [Hilton, M.; Conselice, C. J.] Univ Nottingham, Ctr Astron & Particle Theory, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Roseboom, I. G.; Farrah, D.; Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Burgarella, D.; Buat, V.] Univ Aix Marseille, Lab Astrophys Marseille, OAMP, CNRS, F-13388 Marseille 13, France.
[Berta, S.; Magnelli, B.; Nordon, R.; Popesso, P.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
[Bethermin, M.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu, CNRS,CE Saclay, F-91191 Gif Sur Yvette, France.
[Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France.
[Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Conversi, L.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Magdis, G.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Page, M. J.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Pozzi, F.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Schulz, B.] CALTECH, Ctr Infrared Proc & Anal, JPL, Pasadena, CA 91125 USA.
RP Hilton, M (reprint author), Univ Nottingham, Ctr Astron & Particle Theory, Sch Phys & Astron, Nottingham NG7 2RD, England.
EM matthew.hilton@nottingham.ac.uk
RI Oliver, Seb/A-2479-2013; Conselice, Christopher/B-4348-2013; Hilton,
Matthew James/N-5860-2013; Magdis, Georgios/C-7295-2014;
OI Oliver, Seb/0000-0001-7862-1032; Magdis, Georgios/0000-0002-4872-2294;
Scott, Douglas/0000-0002-6878-9840
FU Leverhulme Trust; STFC; NASA/STScI [HST-GO11082]; CSA (Canada); NAOC
(China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); BMVIT
(Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain)
FX We thank the referee for many helpful comments which have improved this
paper. We thank Amanda Bauer for providing the UV-based SFR measurements
of GNS galaxies and useful discussions. MH and CJC acknowledge financial
support from the Leverhulme Trust and STFC. Support for the GNS was also
provided by NASA/STScI grant HST-GO11082.; 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, UKSA (UK) and
NASA (USA).; PACS has been developed by a consortium of institutes led
by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC
(Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT,
LENS, SISSA (Italy) and IAC (Spain). This development has been supported
by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES
(France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain).
NR 100
TC 10
Z9 10
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2012
VL 425
IS 1
BP 540
EP 555
DI 10.1111/j.1365-2966.2012.21499.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 993VG
UT WOS:000307887300061
ER
PT J
AU MacLachlan, GA
Shenoy, A
Sonbas, E
Dhuga, KS
Eskandarian, A
Maximon, LC
Parke, WC
AF MacLachlan, G. A.
Shenoy, A.
Sonbas, E.
Dhuga, K. S.
Eskandarian, A.
Maximon, L. C.
Parke, W. C.
TI The minimum variability time-scale and its relation to pulse profiles of
Fermi GRBs
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; gamma-ray burst: general
ID GAMMA-RAY BURSTS; LONG; CONJECTURE
AB We present a direct link between the minimum variability time-scales extracted through a wavelet decomposition and the rise times of the shortest pulses extracted via fits of 34 Fermi Gamma-ray Burst Monitor (GBM) Gamma-Ray Burst (GRB) light curves comprised of 379 pulses. Pulses used in this study were fitted with lognormal functions, whereas the wavelet technique used employs a multiresolution analysis that does not rely on identifying distinct pulses. By applying a corrective filter to published data fitted with pulses, we demonstrate agreement between these two independent techniques and offer a method for distinguishing signal from noise.
C1 [MacLachlan, G. A.; Shenoy, A.; Dhuga, K. S.; Eskandarian, A.; Maximon, L. C.; Parke, W. C.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
[Sonbas, E.] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey.
[Sonbas, E.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP MacLachlan, GA (reprint author), George Washington Univ, Dept Phys, Washington, DC 20052 USA.
EM maclach@gwu.edu
FU NASA [NNX11AE36G]
FX The NASA grant NNX11AE36G provided partial support for this work and is
gratefully acknowledged. The authors, in particular GAM and KSD,
acknowledge very useful discussions with Jon Hakkila and Narayan Bhat.
NR 10
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 SEP
PY 2012
VL 425
IS 1
BP L32
EP L35
DI 10.1111/j.1745-3933.2012.01295.x
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 993VG
UT WOS:000307887300012
ER
PT J
AU Link, JS
Ihde, TF
Harvey, CJ
Gaichas, SK
Field, JC
Brodziak, JKT
Townsend, HM
Peterman, RM
AF Link, J. S.
Ihde, T. F.
Harvey, C. J.
Gaichas, S. K.
Field, J. C.
Brodziak, J. K. T.
Townsend, H. M.
Peterman, R. M.
TI Dealing with uncertainty in ecosystem models: The paradox of use for
living marine resource management
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Review
ID COUPLED BIOLOGICAL/PHYSICAL MODELS; SINGLE-SPECIES MODELS;
FISHERIES-MANAGEMENT; SKILL ASSESSMENT; DECISION-MAKING; TIME-SERIES;
CONFLICTING OBJECTIVES; SENSITIVITY ANALYSIS; STOCK ASSESSMENT;
SCIENTIFIC BASIS
AB To better manage living marine resources (LMRs), it has become clear that ecosystem-based fisheries management (EBFM) is a desired approach. To do EBFM, one of the key tools will be to use ecosystem models. To fully use ecosystem models and have their outputs adopted, there is an increasingly recognized need to address uncertainty associated with such modeling activities. Here we characterize uncertainty as applied to ecosystem models into six major factors, including: natural variability; observation error; inadequate communication among scientists, decision-makers and stakeholders; the structural complexity of the model(s) used; outcome uncertainty; and unclear management objectives. We then describe best practices to address each of these uncertainties as they particularly apply to ecosystem models being used in a LMR management context. We also present case studies to highlight examples of how these best practices have been implemented. Although we acknowledge that this work was compiled by ecosystem modelers in an LMR management context primarily for other ecosystem modelers, the principles and practices described herein are also germane for managers, stakeholders and other natural resource management communities. We conclude by emphasizing not only the need to address uncertainty in ecosystem models, but also the feasibility and benefits of doing so. Published by Elsevier Ltd.
C1 [Link, J. S.] Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, Woods Hole, MA 02543 USA.
[Ihde, T. F.; Townsend, H. M.] NOAA, Natl Marine Fisheries Serv, Chesapeake Bay Off, Annapolis, MD 21403 USA.
[Harvey, C. J.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA.
[Gaichas, S. K.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA.
[Field, J. C.] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Santa Cruz, CA 95060 USA.
[Brodziak, J. K. T.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96816 USA.
[Peterman, R. M.] Simon Fraser Univ, Sch Resource & Environm Management, Burnaby, BC V5A 1S6, Canada.
RP Link, JS (reprint author), Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, 166 Water St, Woods Hole, MA 02543 USA.
EM Jason.Link@noaa.gov
NR 135
TC 44
Z9 44
U1 7
U2 63
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 SEP
PY 2012
VL 102
SI SI
BP 102
EP 114
DI 10.1016/j.pocean.2012.03.008
PG 13
WC Oceanography
SC Oceanography
GA 987MP
UT WOS:000307421600008
ER
PT J
AU Zelinski, S
Jastrzebski, M
AF Zelinski, S.
Jastrzebski, M.
TI Defining dynamic route structure for airspace configuration
SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF
AEROSPACE ENGINEERING
LA English
DT Article
DE route structure; airspace configuration; traffic flow; critical points
AB This article describes a method for defining route structure from flight tracks. Individual merge and diverge intersections between pairs of flights are identified, clustered, and grouped into nodes of a route structure network. Links are placed between nodes to represent major traffic flows. A parametric analysis determined the algorithm input parameters producing route structures of current day flight plans that are closest to today's airway structure. These parameters are then used to define and analyse the dynamic route structure over the course of a day for current day flight paths. Route structures are also compared between current day flight paths and more user-preferred paths such as great circle and weather avoidance routing.
C1 [Zelinski, S.] NASA, Aerosp High Dens Operat Branch Code AFH, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Jastrzebski, M.] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, Santa Cruz, CA 95064 USA.
RP Zelinski, S (reprint author), NASA, Aerosp High Dens Operat Branch Code AFH, Ames Res Ctr, Mail Stop 210-15,Bldg 210,Rm 122,POB 1, Moffett Field, CA 94035 USA.
EM shannon.j.zelinski@nasa.gov
FU NASA
FX This study was supported by the NASA Airspace System Program, Concept
and Technology Development Project in support of Dynamic Airspace
Configuration research.
NR 11
TC 2
Z9 2
U1 0
U2 12
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0954-4100
J9 P I MECH ENG G-J AER
JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng.
PD SEP
PY 2012
VL 226
IS G9
BP 1161
EP 1170
DI 10.1177/0954410011417354
PG 10
WC Engineering, Aerospace; Engineering, Mechanical
SC Engineering
GA 992GI
UT WOS:000307763200009
ER
PT J
AU Scott, JM
Martin, DS
Ploutz-Snyder, R
Caine, T
Matz, T
Arzeno, NM
Buxton, R
Ploutz-Snyder, L
AF Scott, Jessica M.
Martin, David S.
Ploutz-Snyder, Robert
Caine, Timothy
Matz, Timothy
Arzeno, Natalia M.
Buxton, Roxanne
Ploutz-Snyder, Lori
TI RELIABILITY AND VALIDITY OF PANORAMIC ULTRASOUND FOR MUSCLE
QUANTIFICATION
SO ULTRASOUND IN MEDICINE AND BIOLOGY
LA English
DT Article
DE Panoramic ultrasound; Magnetic resonance imaging; Cross-sectional area;
Muscle size
ID HUMAN SKELETAL-MUSCLE; CROSS-SECTIONAL AREA; BED REST; VOLUME; EXERCISE;
SIZE
AB This study examined the reliability and validity of using customized templates to acquire panoramic ultrasound (US) images for determining cross-sectional area (CSA) and volume in the vastus lateralis (VL), rectus femoris (RF), medial gastrocnemius (MG) and lateral gastrocnemius (LG). Panoramic US and magnetic resonance imaging (MRI) images were analyzed by two trained investigators. The inter-experimenter reliability (coefficient of variation [CV]) of panoramic US ranged from 2.4% to 4.1% and the intraclass correlation (ICC) ranged from 0.963 to 0.991, whereas the inter-experimenter CV of MRI ranged from 2.8% to 3.8% and the ICC from 0.946 to 0.986. Bland-Altman plots demonstrated high agreement between US and MRI; however, values obtained from MRI were systematically larger than those obtained from US. The present results indicate that using a customized US template provides reliable measures of leg muscle CSA and, thus, could be used to characterize muscle CSA and volume. (E-mail: jessica.m.scott@nasa.gov) (c) 2012 World Federation for Ultrasound in Medicine & Biology.
C1 [Scott, Jessica M.] Univ Space Res Assoc, NASA Johnson Space Ctr, SK, Houston, TX 77058 USA.
[Martin, David S.; Caine, Timothy; Arzeno, Natalia M.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Buxton, Roxanne] Univ Houston, Houston, TX USA.
[Matz, Timothy] MEI Technol, Houston, TX USA.
RP Scott, JM (reprint author), Univ Space Res Assoc, NASA Johnson Space Ctr, SK, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM jessica.m.scott@nasa.gov
FU Human Research Program of the National Aeronautics and Space
Administration (NASA); Natural Sciences and Engineering Research Council
of Canada Post Doctoral Fellowship
FX The authors thank the Flight Analogs Project for the excellent
organization and coordination of the Integrated Resistance and Aerobic
Training Study, as well as the subjects who enthusiastically
participated in the study. This work was supported by the Human Research
Program of the National Aeronautics and Space Administration (NASA) and
a Natural Sciences and Engineering Research Council of Canada Post
Doctoral Fellowship (JMS).
NR 13
TC 10
Z9 10
U1 0
U2 7
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0301-5629
J9 ULTRASOUND MED BIOL
JI Ultrasound Med. Biol.
PD SEP
PY 2012
VL 38
IS 9
BP 1656
EP 1661
DI 10.1016/j.ultrasmedbio.2012.04.018
PG 6
WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
GA 986XC
UT WOS:000307378900022
PM 22749820
ER
PT J
AU Sridharan, D
Wilson, W
Whalen, M
Chappell, L
Cucinotta, F
Pluth, J
AF Sridharan, D.
Wilson, W.
Whalen, M.
Chappell, L.
Cucinotta, F.
Pluth, J.
TI Surrogate Endpoints Reveal Radiation Quality-Dependent Differences in
Mammary Cancer Risk
SO ENVIRONMENTAL AND MOLECULAR MUTAGENESIS
LA English
DT Meeting Abstract
CT 43rd Annual Meeting of the Environmental-Mutagen-Society (EMS)
CY SEP 08-12, 2012
CL Bellevue, WA
SP Environm Mutagen Soc (EMS)
C1 [Sridharan, D.; Wilson, W.; Whalen, M.; Pluth, J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Chappell, L.; Cucinotta, F.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 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 0893-6692
J9 ENVIRON MOL MUTAGEN
JI Environ. Mol. Mutagen.
PD SEP
PY 2012
VL 53
SU 1
BP S42
EP S42
PG 1
WC Environmental Sciences; Genetics & Heredity; Toxicology
SC Environmental Sciences & Ecology; Genetics & Heredity; Toxicology
GA 993YM
UT WOS:000307896300118
ER
PT J
AU Mulenburg, G
AF Mulenburg, Gerald
TI The History of Project Management
SO JOURNAL OF PRODUCT INNOVATION MANAGEMENT
LA English
DT Book Review
C1 [Mulenburg, Gerald] NASA, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 2
U2 12
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0737-6782
J9 J PROD INNOVAT MANAG
JI J. Prod. Innov. Manage.
PD SEP
PY 2012
VL 29
IS 5
BP 898
EP 900
PG 3
WC Business; Engineering, Industrial; Management
SC Business & Economics; Engineering
GA 984BQ
UT WOS:000307164000016
ER
PT J
AU Karaca, HE
Acar, E
Basaran, B
Noebe, RD
Chumlyakov, YI
AF Karaca, H. E.
Acar, E.
Basaran, B.
Noebe, R. D.
Chumlyakov, Y. I.
TI Superelastic response and damping capacity of ultrahigh-strength
[111]-oriented NiTiHfPd single crystals
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Shape memory alloys (SMAs); Phase transformation; Damping; Compression
test; High-strength shape memory alloys
ID SHAPE-MEMORY ALLOYS; MARTENSITIC-TRANSFORMATION; COMPRESSIVE RESPONSE;
CYCLIC DEFORMATION; BEHAVIOR; PSEUDOELASTICITY; HYSTERESIS
AB The superelastic behavior of an NiTiHfPd single-crystal shape memory alloy in compression along the [111] orientation was investigated as a function of temperature. In the range of -30 to 70 degrees C, a perfect superelastic loop with 4.2% transformation strain was attained. In addition, this material exhibited an ultrahigh yield strength of more than 2500 MPa and an exceptional damping capacity of 44 J cm(-3). (C) 2012 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Karaca, H. E.; Acar, E.; Basaran, B.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Chumlyakov, Y. I.] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia.
[Basaran, B.] Univ Houston, Dept Engn Technol, Houston, TX 77024 USA.
RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM karaca@engr.uky.edu
RI yuriy, chumlyakov/C-6033-2009; Chumlyakov, Yuriy/R-6496-2016
FU NASA Fundamental Aeronautics Program; Supersonics Project; NASA EPSCOR
program [NNX11AQ31A]; KY EPSCoR RIDG program [3049024332]; RFBR
[10-03-00154a]
FX This work was supported in part by the NASA Fundamental Aeronautics
Program, Supersonics Project and the NASA EPSCOR program under Grant
nos. NNX11AQ31A, KY EPSCoR RIDG program under Grant no. 3049024332 and
RFBR Project with Grant no. 10-03-00154a.
NR 26
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U1 2
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6462
J9 SCRIPTA MATER
JI Scr. Mater.
PD SEP
PY 2012
VL 67
IS 5
BP 447
EP 450
DI 10.1016/j.scriptamat.2012.05.044
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 987RE
UT WOS:000307434000007
ER
PT J
AU Waliser, DE
Guan, B
Li, JLF
Kim, J
AF Waliser, Duane E.
Guan, Bin
Li, Jui-Lin F.
Kim, Jinwon
TI Addendum to "Simulating cold season snowpack: Impacts of snow albedo and
multi-layer snow physics": Waliser, D., J. Kim, Y. Xue, Y. Chao, A.
Eldering, R. Fovell, A. Hall, Q. Li, K. N. Liou, J. McWilliams, S.
Kapnick, R. Vasic, F. De Sale, and Y. Yu (2011), Climatic Change, 109
(Suppl 1):S95-S117, DOI 10.1007/s10584-011-0312-5
SO CLIMATIC CHANGE
LA English
DT Correction
C1 [Kim, Jinwon] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Waliser, Duane E.; Guan, Bin; Li, Jui-Lin F.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Kim, J (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM jkim@atmos.ucla.edu
RI Guan, Bin/F-6735-2010
NR 1
TC 2
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U1 0
U2 4
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 SEP
PY 2012
VL 114
IS 2
BP 399
EP 400
DI 10.1007/s10584-012-0531-4
PG 2
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 985II
UT WOS:000307256200014
ER
PT J
AU Frazin, RA
Vasquez, AM
Thompson, WT
Hewett, RJ
Lamy, P
Llebaria, A
Vourlidas, A
Burkepile, J
AF Frazin, Richard A.
Vasquez, Alberto M.
Thompson, William T.
Hewett, Russell J.
Lamy, Philippe
Llebaria, Antoine
Vourlidas, Angelos
Burkepile, Joan
TI Intercomparison of the LASCO-C2, SECCHI-COR1, SECCHI-COR2, and Mk4
Coronagraphs
SO SOLAR PHYSICS
LA English
DT Article
DE Coronagraph; Electron density; Solar corona
ID ELECTRON-DENSITY; TOTAL BRIGHTNESS; SOLAR; CALIBRATION; STEREO; MASS;
IMAGES; UVCS
AB In order to assess the reliability and consistency of white-light coronagraph measurements, we report on quantitative comparisons between polarized brightness [pB] and total brightness [B] images taken by the following white-light coronagraphs: LASCO-C2 on SOHO, SECCHI-COR1 and -COR2 on STEREO, and the ground-based MLSO-Mk4. The data for this comparison were taken on 16 April 2007, when both STEREO spacecraft were within 3.1(a similar to) of Earth's heliographic longitude, affording essentially the same view of the Sun for all of the instruments. Due to the difficulties of estimating stray-light backgrounds in COR1 and COR2, only Mk4 and C2 produce reliable coronal-hole values (but not at overlapping heights), and these cannot be validated without rocket flights or ground-based eclipse measurements. Generally, the agreement between all of the instruments' pB values is within the uncertainties in bright streamer structures, implying that measurements of bright CMEs also should be trustworthy. Dominant sources of uncertainty and stray light are discussed, as is the design of future coronagraphs from the perspective of the experiences with these instruments.
C1 [Frazin, Richard A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Vasquez, Alberto M.] UBA, CONICET, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina.
[Vasquez, Alberto M.] UBA, FCEN, Buenos Aires, DF, Argentina.
[Thompson, William T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA.
[Hewett, Russell J.] Univ Illinois, Dept Comp Sci, Urbana, IL 61801 USA.
[Lamy, Philippe; Llebaria, Antoine] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, UMR6110, F-13388 Marseille 13, France.
[Vourlidas, Angelos] USN, Res Lab, Washington, DC 20375 USA.
[Burkepile, Joan] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
RP Frazin, RA (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM rfrazin@umich.edu; albert@iafe.uba.ar; william.t.thompson@nasa.gov;
rhewett@mit.edu; philippe.lamy@oamp.fr; antoine.llebaria@oamp.fr;
iguana@ucar.edu
RI Frazin, Richard/J-2625-2012; Vourlidas, Angelos/C-8231-2009
OI Vourlidas, Angelos/0000-0002-8164-5948
FU NASA Heliophysics Guest Investigator award [NNX08AJ09G]; UBACyT
(Universidad de Buenos Aires) [20020090100264]; NASA under GSRP
fellowship [NNX08AT43H FLL]; Centre National d'Etudes Spatiales (CNES)
FX The authors thank the anonymous referee for helpful comments, which
resulted in a much improved manuscript. This research was supported by
NASA Heliophysics Guest Investigator award NNX08AJ09G to the University
of Michigan. A.M.V. acknowledges UBACyT (Universidad de Buenos Aires)
grant no. 20020090100264 for partial financial support. R.J.H. was
funded by NASA under GSRP fellowship NNX08AT43H FLL. The LASCO-C2
project at Laboratoire d'Astrophysique de Marseille is funded by the
Centre National d'Etudes Spatiales (CNES). The authors thank Katherine
Baldwin for her helpful comments.
NR 28
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U1 1
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2012
VL 280
IS 1
BP 273
EP 293
DI 10.1007/s11207-012-0028-3
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 986OR
UT WOS:000307352700018
ER
PT J
AU Markley, FL
Carpenter, JR
AF Markley, F. Landis
Carpenter, J. Russell
TI Linear Covariance Analysis and Epoch State Estimators
SO JOURNAL OF THE ASTRONAUTICAL SCIENCES
LA English
DT Article
DE Linear covariance analysis; Epoch-state estimator; Consider parameters;
Process noise; Batch least-squares; Kalman filter
AB This paper extends in two directions the results of prior work on generalized linear covariance analysis of both batch least-squares and sequential estimators. The first is an improved treatment of process noise in the batch, or epoch state, estimator with an epoch time that may be later than some or all of the measurements in the batch. The second is to account for process noise in specifying the gains in the epoch state estimator. We establish the conditions under which the latter estimator is equivalent to the Kalman filter.
C1 [Markley, F. Landis] NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Greenbelt, MD 20771 USA.
[Carpenter, J. Russell] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20771 USA.
RP Markley, FL (reprint author), NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Code 591, Greenbelt, MD 20771 USA.
EM Landis.Markley@nasa.gov; Russell.Carpenter@nasa.gov
NR 14
TC 0
Z9 0
U1 0
U2 0
PU AMER ASTRONAUTICAL SOC
PI SPRINGFIELD
PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA
SN 0021-9142
EI 2195-0571
J9 J ASTRONAUT SCI
JI J. Astronaut. Sci.
PD SEP
PY 2012
VL 59
IS 3
BP 585
EP 605
DI 10.1007/s40295-014-0006-0
PG 21
WC Engineering, Aerospace
SC Engineering
GA V35BG
UT WOS:000209125400006
ER
PT J
AU Markley, FL
Carpenter, JR
AF Markley, F. Landis
Carpenter, J. Russell
TI Generalized Linear Covariance Analysis (vol 57, pg 233, 2009)
SO JOURNAL OF THE ASTRONAUTICAL SCIENCES
LA English
DT Correction
C1 [Markley, F. Landis] NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Greenbelt, MD 20771 USA.
[Carpenter, J. Russell] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20771 USA.
RP Markley, FL (reprint author), NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Code 591, Greenbelt, MD 20771 USA.
EM glmarkley@comcast.net; russell.carpenter@nasa.gov
NR 1
TC 1
Z9 1
U1 0
U2 0
PU AMER ASTRONAUTICAL SOC
PI SPRINGFIELD
PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA
SN 0021-9142
EI 2195-0571
J9 J ASTRONAUT SCI
JI J. Astronaut. Sci.
PD SEP
PY 2012
VL 59
IS 3
BP 606
EP 607
DI 10.1007/s40295-014-0015-z
PG 2
WC Engineering, Aerospace
SC Engineering
GA V35BG
UT WOS:000209125400007
ER
PT J
AU Russell, CT
Grotzinger, JP
Vasavada, AR
AF Russell, C. T.
Grotzinger, John P.
Vasavada, Ashwin R.
TI Preface
SO SPACE SCIENCE REVIEWS
LA English
DT Editorial Material
C1 [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
[Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Russell, CT (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
EM ctrussel@igpp.ucla.edu
RI Russell, Christopher/E-7745-2012
OI Russell, Christopher/0000-0003-1639-8298
NR 0
TC 5
Z9 5
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2012
VL 170
IS 1-4
BP 1
EP 2
DI 10.1007/s11214-012-9928-7
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 008JF
UT WOS:000308952500001
ER
PT J
AU Johansson, ML
Sremba, AL
Feinberg, LR
Banks, MA
Peterson, WT
AF Johansson, Mattias L.
Sremba, Angela L.
Feinberg, Leah R.
Banks, Michael A.
Peterson, William T.
TI The mitochondrial genomes of Euphausia pacifica and Thysanoessa raschii
sequenced using 454 next-generation sequencing, with a phylogenetic
analysis of their position in the Malacostracan family tree
SO MOLECULAR BIOLOGY REPORTS
LA English
DT Article
DE mtDNA; Mitochondrial genome; Phylogeny; Malacostraca; Euphausiacea
ID UNIQUE GENE ORDER; ANTARCTIC KRILL; CONTROL REGION; DNA SEQUENCE;
DECAPOD CRUSTACEANS; SPINY LOBSTER; CRAB; BRACHYURA; SUPERBA; AMPHIPODA
AB Euphausiid krill play a critical role in coastal and oceanic food webs, linking primary producers to upper trophic levels. In addition, some species support commercial fisheries worldwide. Despite their ecological importance, the genetics of these important species remain poorly described. To improve our understanding of the genetics of these ecological links, we sequenced the mitochondrial genomes of two species of North Pacific krill, Euphausia pacifica and Thysanoessa raschii, using long-range PCR and 454 GS Junior next-generation sequencing technology. The E. pacifica mitogenome (14,692 + base pairs (bp)) encodes 13 protein-coding genes (PCGs), two ribosomal RNA (rRNA) genes, and at least 22 transfer RNA (tRNA) genes. The T. raschii mitogenome (14,240 + bp) encodes 13 PCGs, two rRNA genes, and at least 19 tRNA genes. The gene order in both species is similar to that of E. superba. Comparisons between Bering Sea and Yellow Sea E. pacifica revealed a total of 644 variable sites. The most variable protein-coding gene were atp8 (7.55 %, 12 of 159 sites variable), nad4 (6.35 %, 85 variable sites) and nad6 (6.32 %, 33 variable sites). Phylogenetic analyses to assess the phylogenetic position of the Euphausiacea, using the concatenated nucleic acid sequences of E. pacifica and T. raschii along with 46 previously published malacostracan mitogenomes, support the monophyly of the order Decapoda and indicate that the Euphausiacea share a common ancestor with the Decapoda. Future research should utilize this sequence data to explore the population genetics and molecular ecology of these species.
C1 [Johansson, Mattias L.; Sremba, Angela L.; Feinberg, Leah R.; Banks, Michael A.] Oregon State Univ, Cooperat Inst Marine Resources Studies, Newport, OR USA.
[Banks, Michael A.] Oregon State Univ, Dept Fisheries & Wildlife, Coastal Oregon Marine Expt Stn, Corvallis, OR 97331 USA.
[Peterson, William T.] NOAA, Hatfield Marine Sci Ctr, Natl Marine Fisheries Serv, Newport, OR USA.
RP Johansson, ML (reprint author), Oregon State Univ, Cooperat Inst Marine Resources Studies, Newport, OR USA.
EM mattias.johansson@oregonstate.edu
RI Johansson, Mattias/F-1049-2011
OI Johansson, Mattias/0000-0003-3042-750X
FU NOAA [NA06NMF4550286]
FX This work was supported by a NOAA award to CIMRS (Award No.
NA06NMF4550286). The authors also gratefully acknowledge O. Drechsel for
assistance with constructing genome maps with OGDRAW, B. Slikas, D.
Steel, A. Alexander, and D. Jacobson for assistance with 454 sequencing,
and T. Shaw, J. Peterson, J. Menkel, and J. Fisher for krill sample
collection. The manuscript was greatly improved by the advice of two
anonymous reviewers.
NR 54
TC 3
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U1 0
U2 32
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0301-4851
J9 MOL BIOL REP
JI Mol. Biol. Rep.
PD SEP
PY 2012
VL 39
IS 9
BP 9009
EP 9021
DI 10.1007/s11033-012-1772-z
PG 13
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA 979EX
UT WOS:000306799700054
PM 22733485
ER
PT J
AU Narkawicz, A
Munoz, C
Dowek, G
AF Narkawicz, Anthony
Munoz, Cesar
Dowek, Gilles
TI Provably correct conflict prevention bands algorithms
SO SCIENCE OF COMPUTER PROGRAMMING
LA English
DT Article
DE Formal verification; Theorem proving; Air traffic management
AB In air traffic management, a pairwise conflict is a predicted loss of separation between two aircraft, referred to as the ownship and the intruder. A conflict prevention bands system displays ranges of maneuvers for the ownship that characterize regions in the airspace that are either conflict-free or "don't go" zones that the ownship has to avoid. Errors in the calculation of prevention bands may result in incorrect separation assurance information being displayed to pilots or air traffic controllers. Algorithms that compute conflict prevention bands are surprisingly difficult to formalize and verify. This paper presents a method for the analysis and verification of prevention bands algorithms. The method, which has been implemented in the Prototype Verification System (PVS), is illustrated with a provably correct 3-dimensional (3D) prevention bands algorithm for track angle maneuvers. Published by Elsevier B.V.
C1 [Narkawicz, Anthony; Munoz, Cesar] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Dowek, Gilles] Ecole Polytech, F-91128 Palaiseau, France.
RP Munoz, C (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM cesar.a.munoz@nasa.gov
NR 14
TC 4
Z9 4
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-6423
J9 SCI COMPUT PROGRAM
JI Sci. Comput. Program.
PD SEP 1
PY 2012
VL 77
IS 10-11
SI SI
BP 1039
EP 1057
DI 10.1016/j.scico.2011.07.002
PG 19
WC Computer Science, Software Engineering
SC Computer Science
GA 980JQ
UT WOS:000306889800002
ER
PT J
AU Kishtawal, CM
Niyogi, D
Kumar, A
Bozeman, ML
Kellner, O
AF Kishtawal, Chandra M.
Niyogi, Dev
Kumar, Anil
Bozeman, Monica Laureano
Kellner, Olivia
TI Sensitivity of inland decay of North Atlantic tropical cyclones to soil
parameters
SO NATURAL HAZARDS
LA English
DT Article
DE Tropical cyclone; Land-falling cyclones; Hurricane intensity; Land
surface feedback; Soil heat flux; Inland decay
ID GENETIC ALGORITHMS; EMPIRICAL-MODEL; WIND-SPEED; LANDFALL; INTENSITY;
SEA
AB Using the HURDAT best track analysis of track and intensity of tropical cyclones that made landfall over the continental United States during the satellite era (1980-2005), we analyze the role of land surface variables on the cyclone decay process. The land surface variables considered in the present study included soil parameters (soil heat capacity and its surrogate soil bulk density), roughness, topography and local gradients of topography. The sensitivity analysis was carried out using a data-adaptive genetic algorithm approach that automatically selects the most suitable variables by fitting optimum empirical functions that estimates cyclone intensity decay in terms of given observed variables. Analysis indicates that soil bulk density (soil heat capacity) has a dominant influence on cyclone decay process. The decayed inland cyclone intensities were found to be positively correlated with the cube of the soil bulk density (heat capacity). The impact of the changes in soil bulk density (heat capacity) on the decayed cyclone intensity is higher for higher intensity cyclones. Since soil bulk density is closely related to the soil heat capacity and inversely proportional to the thermal diffusivity, the observed relationship can also be viewed as the influence of cooling rate of the land surface, as well as the transfer of heat and moisture underneath a land-falling storm. The optimized prediction function obtained by statistical model processes in the present study that predicts inland intensity changes during 6-h interval showed high fitness index and small errors. The performance of the prediction function was tested on inland tracks of eighteen hurricanes and tropical storms that made landfall over the United States between 2001 and 2010. The mean error of intensity prediction for these cyclones varied from 1.3 to 15.8 knots (0.67-8.12 m s(-1)). Results from the data-driven analysis thus indicate that soil heat flux feedback should be an important consideration for the inland decay of tropical cyclones. Experiments were also undertaken using Weather Research Forecasting (WRF) Advanced Research Version (ARW ver 3.3) to assess the sensitivity of the soil parameters (roughness, heat capacity and bulk density) on the post-landfall structure of select storms. The model was run with 1-km grid spacing, limited area single domain with boundary conditions from the North American Regional Reanalysis. Of different experiments, only the surface roughness change and soil bulk density (heat capacity) change experiments showed some sensitivity to the intensity change. The WRF results thus have a low sensitivity to the land parameters (with only the roughness length showing some impact). This calls for reassessing the land surface response on post-landfall characteristics with more detailed land surface representation within the mesoscale and hurricane modeling systems.
C1 [Kishtawal, Chandra M.; Niyogi, Dev; Bozeman, Monica Laureano; Kellner, Olivia] Purdue Univ, W Lafayette, IN 47906 USA.
[Kishtawal, Chandra M.] ISRO, SAC, Ahmadabad 380015, Gujarat, India.
[Kumar, Anil] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
[Kumar, Anil] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Niyogi, D (reprint author), Purdue Univ, W Lafayette, IN 47906 USA.
EM climate@purdue.edu
NR 31
TC 5
Z9 5
U1 3
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0921-030X
J9 NAT HAZARDS
JI Nat. Hazards
PD SEP
PY 2012
VL 63
IS 3
BP 1527
EP 1542
DI 10.1007/s11069-011-0015-2
PG 16
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA 976MS
UT WOS:000306589500014
ER
PT J
AU Kellner, O
Niyogi, D
Lei, M
Kumar, A
AF Kellner, Olivia
Niyogi, Dev
Lei, Ming
Kumar, Anil
TI The role of anomalous soil moisture on the inland reintensification of
Tropical Storm Erin (2007)
SO NATURAL HAZARDS
LA English
DT Article
DE Tropical Storm Erin; Storm reintensification; Storm intensity; Land
surface processes; Soil moisture; Landfalling cyclones
ID EXTRATROPICAL TRANSITION; ENVIRONMENTAL-INFLUENCES; SURFACE-TEMPERATURE;
HURRICANE INTENSITY; FEEDBACK MECHANISM; RAINFALL FEEDBACK; CYCLONE
STRUCTURE; NUMERICAL-MODEL; BOUNDARY-LAYER; GREAT-PLAINS
AB Prior research on tropical storm systems that have made landfall and undergone a period of sustainability or reintensification has been linked to the synoptic environment at the time the storm restrengthened. Tropical Storm (TS) Erin is an interesting case study in that it did not take on hurricane-like structure nor reach hurricane intensity until it moved through west-central Oklahoma on August 19, 2007. This study seeks to examine the possible impact of anomalously wet soils across much of Oklahoma on the reintensification of TS Erin during the early morning hours of August 19, 2007. To determine the degree to which the antecedent soil state impacted TS Erin's inland evolution and reintensification, analyses of the synoptic environment and the mesoscale environment/boundary layer environment are undertaken using operational and research datasets such as upper air soundings, surface soil moisture and temperature data, and multiple products from the Storm Prediction Center (SPC) mesoanalysis archive. This observational assessment is complemented with numerical experiments using the Weather Research and Forecast Model, Advanced Research Version 3.2 (WRF-ARW) to further study the role of soil moisture availability and surface fluxes that may have led to the boundary layer feedback and inland reintensification. Observational analysis and model results indicate that anomalously wet conditions over the central Oklahoma region may have helped develop a regional boundary layer feedback that appears to have contributed to the inland reintensification of TS Erin. Thus, the anomalously wet land surface had a positive role in TS Erin reintensifying over Oklahoma during the early morning hours of August 19, 2007.
C1 [Kellner, Olivia; Niyogi, Dev; Lei, Ming] Purdue Univ, Indiana State Climate Off, W Lafayette, IN 47907 USA.
[Kumar, Anil] NASA, GSFC, Hydrol Sci Branch, College Pk, MD USA.
[Kumar, Anil] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
RP Kellner, O (reprint author), Purdue Univ, Indiana State Climate Off, LILY 2-420,915 State St, W Lafayette, IN 47907 USA.
EM okellner@purdue.edu; dniyogi@purdue.edu
FU NASA; DOE-ARM [08ER64674]
FX Study benefited in part from NASA Earth and Space Science Fellowship
(Dr. W. W. Wang), and the DOE-ARM 08ER64674 (Dr. Rick Petty), and
discussions with Prof. Marshall Shepherd at the University of Georgia,
and Dr. Jeff Basara at the University of Oklahoma. Special thanks are
given to Dr. Michael Baldwin and Dr. Jonathon Harbor of Purdue
University and to Daniel McCarthy of the Indianapolis National Weather
Service for continued feedback and support of the research project.
NR 48
TC 7
Z9 7
U1 4
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0921-030X
J9 NAT HAZARDS
JI Nat. Hazards
PD SEP
PY 2012
VL 63
IS 3
BP 1573
EP 1600
DI 10.1007/s11069-011-9966-6
PG 28
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA 976MS
UT WOS:000306589500016
ER
PT J
AU Singh, HB
Cai, C
Kaduwela, A
Weinheimer, A
Wisthaler, A
AF Singh, H. B.
Cai, C.
Kaduwela, A.
Weinheimer, A.
Wisthaler, A.
TI Interactions of fire emissions and urban pollution over California:
Ozone formation and air quality simulations
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Ozone; Wildfires; Urban pollution; Nitrogen oxides; PAN; Formaldehyde;
Aerosol
ID HIGH NORTHERN LATITUDES; RUSSIAN WILDFIRES; EASTERN FINLAND; MODEL;
AIRCRAFT; AEROSOLS; TROPOSPHERE; ATMOSPHERE; BOREAL; FOREST
AB An instrumented DC-8 aircraft was employed to perform airborne observations in rural and urban environs of California during the summer 2008 NASA ARCTAS-CARB campaign. The fortuitous occurrence of large wildfire episodes in Northern California allowed for studies of fire emissions, their composition, and their interactions with rural and urban air. Relative to CO, emissions of HCN were shown to vary non-linearly with fire characteristics while those of CH3CN were nearly unchanged, making the latter a superior quantitative tracer of biomass combustion. Although some fire plumes over California contained little NOx and virtually no O-3 enhancement, others contained ample VOCs and sufficient NOx, largely from urban influences, to result in significant ozone formation. The highest observed O-3 mixing ratios (170 ppb) were also in fire-influenced urban air masses. Attempts to simulate these interactions using CMAQ a high-resolution state of the art air quality model, were only minimally successful and indicated several shortcomings in simulating fire emission influences on urban smog formation. A variety of secondary oxidation products (e.g. O-3, PAN, HCHO) were substantially underestimated in fire-influenced air masses. Available data involving fire plumes and anthropogenic pollution interactions are presently quite sparse and additional observational and mechanistic studies are needed. Published by Elsevier Ltd.
C1 [Singh, H. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cai, C.; Kaduwela, A.] Calif Air Resources Board, Sacramento, CA USA.
[Weinheimer, A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Wisthaler, A.] Univ Innsbruck, A-6020 Innsbruck, Austria.
RP Singh, HB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Hanwant.b.singh@nasa.gov
OI Kaduwela, Ajith/0000-0002-7236-2698
FU NASA Tropospheric Chemistry Program; California Air Resources Board;
Austrian Research Promotion Agency (FFG-ALR); Tiroler Zukunftstiftung;
NASA Radiation Sciences Program
FX The ARCTAS-CARB campaign was funded by the NASA Tropospheric Chemistry
Program, the NASA Radiation Sciences Program, and the California Air
Resources Board. CH3CN measurements were supported by the
Austrian Research Promotion Agency (FFG-ALR) and the Tiroler
Zukunftstiftung. PAN and formaldehyde data are due to G. Huey (Georgia
Tech) and A. Fried (NCAR), respectively. We thank all ARCTAS-CARB
participants for their support and contributions.
NR 40
TC 25
Z9 25
U1 9
U2 63
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2012
VL 56
BP 45
EP 51
DI 10.1016/j.atmosenv.2012.03.046
PG 7
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 973GK
UT WOS:000306347900006
ER
PT J
AU Liu, SY
Ding, W
Gao, F
Stepinski, TF
AF Liu, Siyi
Ding, Wei
Gao, Feng
Stepinski, Tomasz F.
TI Adaptive Selective Learning for automatic identification of
sub-kilometer craters
SO NEUROCOMPUTING
LA English
DT Article
DE Pattern recognition; Active learning; Semi-supervised learning; Crater
detection; Mars
ID MARS; CHRONOLOGY
AB Counting craters is a fundamental task of planetary science, because it provides the only tool for measuring relative ages of planetary surfaces. However, advances in surveying craters present in data gathered by planetary probes have not kept up with advances in data collection. It becomes extremely challenging to automatically count a very large number of small, sub-kilometer size craters in a deluge of high resolution planetary images. In this paper, we combine active learning with semi-supervised learning to build an adaptive learning system to automatically detect craters from high resolution panchromatic planetary images. We propose an Adaptive Selective Algorithm to iteratively enrich an original small training set, using unlabeled test set without additional human labeling effort, to detect craters from a large volume of images. We propose three strategies to improve detection accuracy by integrating classification with exploration on unlabeled samples. The Majority Vote Strategy is used to automatically obtain class labels by exploiting unlabeled samples. The De-Mixed Strategy is used on instance filtering to obtain reliable samples. The Active Stability Strategy is used to obtain an appropriate class distribution in the constructed training set by detecting unstable classes. By using those three strategies, we actively select test instances from test images into an existing small initial training set while rebuilding the classifier in the mean time. Our proposed algorithms are empirically evaluated on a large high resolution Martian image, exhibiting a heavily cratered Martian terrain characterized by heterogeneous surface morphology. The experimental results demonstrate that the proposed approach achieves a higher accuracy than other existing approaches to a large extent. (c) 2012 Elsevier B.V. All rights reserved.
C1 [Liu, Siyi; Ding, Wei] Univ Massachusetts, Dept Comp Sci, Boston, MA 02125 USA.
[Gao, Feng] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Stepinski, Tomasz F.] Univ Cincinnati, Dept Geog, Cincinnati, OH 45221 USA.
RP Ding, W (reprint author), Univ Massachusetts, Dept Comp Sci, Harbor Campus, Boston, MA 02125 USA.
EM sliu@cs.umb.edu; ding@cs.umb.edu; feng.gao-1@nasa.gov; stepintz@uc.edu
FU NASA grant [NNX09AK86G]
FX This work was partially supported by the NASA grant NNX09AK86G. The
authors would like to thank Ph.D. students Yang Mu and William Isaac
Miller of the Knowledge Discovery Lab., Computer Science Department,
University of Massachusetts Boston for informative discussions on the
algorithm design.
NR 34
TC 3
Z9 3
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0925-2312
EI 1872-8286
J9 NEUROCOMPUTING
JI Neurocomputing
PD SEP 1
PY 2012
VL 92
SI SI
BP 78
EP 87
DI 10.1016/j.neucom.2011.11.023
PG 10
WC Computer Science, Artificial Intelligence
SC Computer Science
GA 963YB
UT WOS:000305659800011
ER
PT J
AU Houweling, S
Badawy, B
Baker, DF
Basu, S
Belikov, D
Bergamaschi, P
Bousquet, P
Broquet, G
Butler, T
Canadell, JG
Chen, J
Chevallier, F
Ciais, P
Collatz, GJ
Denning, S
Engelen, R
Enting, IG
Fischer, ML
Fraser, A
Gerbig, C
Gloor, M
Jacobson, AR
Jones, DBA
Heimann, M
Khalil, A
Kaminski, T
Kasibhatla, PS
Krakauer, NY
Krol, M
Maki, T
Maksyutov, S
Manning, A
Meesters, A
Miller, JB
Palmer, PI
Patra, P
Peters, W
Peylin, P
Poussi, Z
Prather, MJ
Randerson, JT
Rockmann, T
Rodenbeck, C
Sarmiento, JL
Schimel, DS
Scholze, M
Schuh, A
Suntharalingam, P
Takahashi, T
Turnbull, J
Yurganov, L
Vermeulen, A
AF Houweling, Sander
Badawy, Bakr
Baker, David F.
Basu, Sourish
Belikov, Dmitry
Bergamaschi, Peter
Bousquet, Philippe
Broquet, Gregoire
Butler, Tim
Canadell, Josep G.
Chen, Jing
Chevallier, Frederic
Ciais, Philippe
Collatz, G. James
Denning, Scott
Engelen, Richard
Enting, Ian G.
Fischer, Marc L.
Fraser, Annemarie
Gerbig, Christoph
Gloor, Manuel
Jacobson, Andrew R.
Jones, Dylan B. A.
Heimann, Martin
Khalil, Aslam
Kaminski, Thomas
Kasibhatla, Prasad S.
Krakauer, Nir Y.
Krol, Maarten
Maki, Takashi
Maksyutov, Shamil
Manning, Andrew
Meesters, Antoon
Miller, John B.
Palmer, Paul I.
Patra, Prabir
Peters, Wouter
Peylin, Philippe
Poussi, Zegbeu
Prather, Michael J.
Randerson, James T.
Rockmann, Thomas
Rodenbeck, Christian
Sarmiento, Jorge L.
Schimel, David S.
Scholze, Marko
Schuh, Andrew
Suntharalingam, Parv
Takahashi, Taro
Turnbull, Jocelyn
Yurganov, Leonid
Vermeulen, Alex
TI Iconic CO2 Time Series at Risk
SO SCIENCE
LA English
DT Letter
C1 [Houweling, Sander; Basu, Sourish; Krol, Maarten] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Houweling, Sander; Basu, Sourish; Krol, Maarten; Rockmann, Thomas] Inst Marine & Atmospher Res Utrecht, NL-3584 CC Utrecht, Netherlands.
[Badawy, Bakr; Gerbig, Christoph; Heimann, Martin; Rodenbeck, Christian] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
[Baker, David F.; Denning, Scott; Schuh, Andrew] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Belikov, Dmitry; Maksyutov, Shamil] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
[Bergamaschi, Peter] European Commiss Joint Res Ctr, Ispra, Italy.
[Bousquet, Philippe; Broquet, Gregoire; Chevallier, Frederic; Ciais, Philippe; Peylin, Philippe] CNRS, UVSQ, Unite Mixte CEA, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
[Butler, Tim] Inst Adv Sustainabil Studies, D-14467 Potsdam, Germany.
[Canadell, Josep G.] CSIRO, Global Carbon Project, Canberra, ACT 2601, Australia.
[Chen, Jing; Jones, Dylan B. A.] Univ Toronto, Toronto, ON M5S 1A7, Canada.
[Collatz, G. James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Engelen, Richard] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Enting, Ian G.] Univ Melbourne, ARC Ctr Excellence Math & Stat Complex Syst, Melbourne, Vic 3010, Australia.
[Fischer, Marc L.] Lawrence Berkeley Natl Lab, Washington, DC 20024 USA.
[Fraser, Annemarie; Palmer, Paul I.] Univ Edinburgh, Edinburgh EH9 3JW, Midlothian, Scotland.
[Gloor, Manuel] Univ Leeds, Earth & Biosphere Inst, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
[Jacobson, Andrew R.; Miller, John B.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Jacobson, Andrew R.; Miller, John B.] NOAA Earth Syst Res Lab, Boulder, CO 80305 USA.
[Khalil, Aslam] Portland State Univ, Portland, OR 97207 USA.
[Kaminski, Thomas] FastOpt, D-22767 Hamburg, Germany.
[Kasibhatla, Prasad S.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Krakauer, Nir Y.] CUNY City Coll, Dept Civil Engn, New York, NY 10031 USA.
[Krol, Maarten; Peters, Wouter] Univ Wageningen & Res Ctr, NL-6708 PB Wageningen, Netherlands.
[Maki, Takashi] Meteorol Res Inst, Environm & Appl Meteorol Res Dept, Tsukuba, Japan.
[Manning, Andrew; Suntharalingam, Parv] Univ E Anglia, Norwich NR4 7TJ, Norfolk, England.
[Meesters, Antoon] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Patra, Prabir] Japan Agcy Marine Earth Sci & Technol, Res Inst Global Change, Yokohama, Kanagawa 2360001, Japan.
[Poussi, Zegbeu] ClimMod, F-91401 Orsay, France.
[Prather, Michael J.; Randerson, James T.] Univ Calif Irvine, Irvine, CA 92697 USA.
[Sarmiento, Jorge L.] Princeton Univ, Princeton, NJ 08544 USA.
[Schimel, David S.] Natl Ecol Observ Inc, Boulder, CO 80301 USA.
[Scholze, Marko] Univ Bristol, Clifton BS8 1RJ, England.
[Takahashi, Taro] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Turnbull, Jocelyn] GNS Sci, Natl Isotope Ctr, Lower Hutt, New Zealand.
[Yurganov, Leonid] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Vermeulen, Alex] Energieonderzoek Ctr Nederland, NL-1755 ZG Petten, Netherlands.
RP Houweling, S (reprint author), SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
EM s.houweling@sron.nl
RI Fraser, Annemarie/D-3874-2012; collatz, george/D-5381-2012; Gerbig,
Christoph/L-3532-2013; Peters, Wouter/B-8305-2008; Krol,
Maarten/E-3414-2013; Scholze, Marko/N-4573-2014; Jones,
Dylan/O-2475-2014; Palmer, Paul/F-7008-2010; Maksyutov,
Shamil/G-6494-2011; Vermeulen, Alex/A-2867-2015; Rockmann,
Thomas/F-4479-2015; Canadell, Josep/E-9419-2010; Vuichard,
Nicolas/A-6629-2011; Chevallier, Frederic/E-9608-2016; Heimann,
Martin/H-7807-2016; Belikov, Dmitry/I-9877-2016; Manning,
Andrew/D-4416-2011;
OI Gerbig, Christoph/0000-0002-1112-8603; Peters,
Wouter/0000-0001-8166-2070; Scholze, Marko/0000-0002-3474-5938; Jones,
Dylan/0000-0002-1935-3725; Maksyutov, Shamil/0000-0002-1200-9577;
Vermeulen, Alex/0000-0002-8158-8787; Rockmann,
Thomas/0000-0002-6688-8968; Canadell, Josep/0000-0002-8788-3218;
Chevallier, Frederic/0000-0002-4327-3813; Heimann,
Martin/0000-0001-6296-5113; Manning, Andrew/0000-0001-6952-7773;
Belikov, Dmitry/0000-0002-2114-7250
NR 7
TC 6
Z9 6
U1 4
U2 65
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 31
PY 2012
VL 337
IS 6098
BP 1038
EP 1040
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 996WP
UT WOS:000308125800018
PM 22936755
ER
PT J
AU Ao, CO
Waliser, DE
Chan, SK
Li, JL
Tian, BJ
Xie, FQ
Mannucci, AJ
AF Ao, Chi O.
Waliser, Duane E.
Chan, Steven K.
Li, Jui-Lin
Tian, Baijun
Xie, Feiqin
Mannucci, Anthony J.
TI Planetary boundary layer heights from GPS radio occultation refractivity
and humidity profiles
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LOWER TROPOSPHERE; SIGNALS; TOP; PACIFIC; DEPTH; PARAMETERIZATION;
STRATOCUMULUS; ATMOSPHERE; INVERSION; MODELS
AB The height of the planetary boundary layer (PBL) is an important parameter that relates to the various processes associated with the PBL. In this paper, we use Global Positioning System radio occultation (GPSRO) measurements to derive a global climatology of PBL heights. Utilizing the strength of GPSRO in capturing fine vertical structures, the top of the PBL is defined to be the height at which the vertical gradient of the refractivity or water vapor partial pressure is minimum, corresponding to the height where the refractivity or water vapor pressure changes most rapidly. A "sharpness parameter" is defined that quantifies the applicability of these definitions. The sharpness parameter is largest over the subtropical regions characterized by strong subsidence. When the sharpness parameter is large, the refractivity-and moisture-based heights are shown to converge. We derived global PBL height climatology using three years (Dec. 2006-Nov. 2009) of COSMIC/FORMOSAT-3 measurements and compared with values calculated from ECMWF Reanalysis Interim (ERA-Int). We found that the mean PBL heights from GPSRO shared similar spatial and seasonal variations with ERA-Int; however, GPSRO heights were higher by 500 m. The standard deviation was also higher from GPSRO, especially in the tropics. We present detailed comparisons between GPSRO and ERA-Int over the Pacific Ocean and the Sahara desert and examine the PBL height distributions as well as its annual and diurnal variabilities. These results suggest that the underlying causes of the bias between GPSRO and ERA-Int likely vary from region to region.
C1 [Ao, Chi O.; Waliser, Duane E.; Chan, Steven K.; Li, Jui-Lin; Tian, Baijun; Xie, Feiqin; Mannucci, Anthony J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Xie, Feiqin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Ao, CO (reprint author), CALTECH, Jet Prop Lab, M-S 138-308,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM chi.o.ao@jpl.nasa.gov
RI Tian, Baijun/A-1141-2007; XIE, FEIQIN/J-4569-2013;
OI Tian, Baijun/0000-0001-9369-2373; Xie, Feiqin/0000-0002-3936-9759
NR 46
TC 28
Z9 29
U1 0
U2 28
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 30
PY 2012
VL 117
AR D16117
DI 10.1029/2012JD017598
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 999NL
UT WOS:000308320400001
ER
PT J
AU Cook, BI
Bell, AR
Anchukaitis, KJ
Buckley, BM
AF Cook, B. I.
Bell, A. R.
Anchukaitis, K. J.
Buckley, B. M.
TI Snow cover and precipitation impacts on dry season streamflow in the
Lower Mekong Basin
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RIVER-BASIN; CLIMATE; WATER; VARIABILITY; ENVIRONMENT
AB Climate change impacts on dry season streamflow in the Mekong River are relatively understudied, despite the fact that water availability during this time is critically important for agricultural and ecological systems. Analyses of two gauging stations (Vientiane and Kratie) in the Lower Mekong Basin (LMB) show significant positive correlations between dry season (March through May, MAM) discharge and upper basin snow cover and local precipitation. Using snow cover, precipitation, and upstream discharge as predictors, we develop skillful regression models for MAM streamflow at Vientiane and Kratie, and force these models with output from a suite of general circulation model (GCM) experiments for the twentieth and twenty-first centuries. The GCM simulations predict divergent trends in snow cover (decreasing) and precipitation (increasing) over the twenty-first century, driving overall negligible long-term trends in dry season streamflow. Our study demonstrates how future changes in dry season streamflow in the LMB will depend on changes in snow cover and precipitation, factors that will need to be considered when assessing the full basin response to other climatic and non-climatic drivers.
C1 [Cook, B. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Cook, B. I.; Anchukaitis, K. J.; Buckley, B. M.] Lamont Doherty Earth Observ, Palisades, NY USA.
[Bell, A. R.] Int Food Policy Res Inst, Washington, DC 20036 USA.
RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM benjamin.i.cook@nasa.gov
RI Cook, Benjamin/H-2265-2012;
OI Anchukaitis, Kevin/0000-0002-8509-8080; Bell, Andrew/0000-0002-1164-312X
FU Greater Mekong Basin Project (NSF Coupled Human and Natural Systems)
[GEO 0908971]
FX This work was supported by the Greater Mekong Basin Project (NSF Coupled
Human and Natural Systems, GEO 0908971). Snow cover data were provided
by Thomas Estilow and the Rutgers University Snow Lab. The authors
gratefully acknowledge the Mekong River Commission (Peter Adamson and
Erland Jensen) for providing the monthly Mekong River discharge data.
Three anonymous reviewers provided comments that greatly improved the
quality of this manuscript. We acknowledge the World Climate Research
Programme's Working Group on Coupled Modeling, which is responsible for
CMIP, and we thank the climate modeling groups for producing and making
available their model output. For CMIP, the U.S. Department of Energy's
Program for Climate Model Diagnosis and Intercomparison provides
coordinating support and led development of software infrastructure in
partnership with the Global Organization for Earth System Science
Portals. Lamont contribution 7577.
NR 41
TC 4
Z9 4
U1 1
U2 7
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 30
PY 2012
VL 117
AR D16116
DI 10.1029/2012JD017708
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 999NL
UT WOS:000308320400002
ER
PT J
AU McGrath, D
Steffen, K
Rajaram, H
Scambos, T
Abdalati, W
Rignot, E
AF McGrath, Daniel
Steffen, Konrad
Rajaram, Harihar
Scambos, Ted
Abdalati, Waleed
Rignot, Eric
TI Basal crevasses on the Larsen C Ice Shelf, Antarctica: Implications for
meltwater ponding and hydrofracture
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID BREAK-UP; PENINSULA; COLLAPSE; STABILITY; CLIMATE; GLACIERS;
DISINTEGRATION; CAPSIZE; SHEET
AB A key mechanism for the rapid collapse of both the Larsen A and B Ice Shelves was meltwater-driven crevasse propagation. Basal crevasses, large-scale structural features within ice shelves, may have contributed to this mechanism in three important ways: i) the shelf surface deforms due to modified buoyancy and gravitational forces above the basal crevasse, creating >10 m deep compressional surface depressions where meltwater can collect, ii) bending stresses from the modified shape drive surface crevassing, with crevasses reaching 40 m in width, on the flanks of the basal-crevasse-induced trough and iii) the ice thickness is substantially reduced, thereby minimizing the propagation distance before a full-thickness rift is created. We examine a basal crevasse (4.5 km in length, similar to 230 m in height), and the corresponding surface features, in the Cabinet Inlet sector of the Larsen C Ice Shelf using a combination of high-resolution (0.5 m) satellite imagery, kinematic GPS and in situ ground penetrating radar. We discuss how basal crevasses may have contributed to the breakup of the Larsen B Ice Shelf by directly controlling the location of meltwater ponding and highlight the presence of similar features on the Amery and Getz Ice Shelves with high-resolution imagery. Citation: McGrath, D., K. Steffen, H. Rajaram, T. Scambos, W. Abdalati, and E. Rignot (2012), Basal crevasses on the Larsen C Ice Shelf, Antarctica: Implications for meltwater ponding and hydrofracture, Geophys. Res. Lett., 39, L16504, doi:10.1029/2012GL052413.
C1 [McGrath, Daniel; Steffen, Konrad; Abdalati, Waleed] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Rajaram, Harihar] Univ Colorado, Dept Civil Engn, Boulder, CO 80309 USA.
[Scambos, Ted] Univ Colorado, Natl Snow & Ice Data Ctr CIRES, Boulder, CO 80309 USA.
[Abdalati, Waleed] NASA Headquarters, Washington, DC USA.
[Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP McGrath, D (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM daniel.mcgrath@colorado.edu
RI Rignot, Eric/A-4560-2014; Steffen, Konrad/C-6027-2013;
OI Rignot, Eric/0000-0002-3366-0481; Steffen, Konrad/0000-0001-8658-1026;
MCGRATH, DANIEL/0000-0002-9462-6842
FU NSF OPP research grant [0732946]; Polar Geospatial Center under NSF OPP
[ANT-1043681]
FX This work is funded by NSF OPP research grant 0732946. The British
Antarctic Survey and field assistant, Tom Weston, provided exceptional
field support, without which this work would not have been possible.
Geospatial support for this work was supported by the Polar Geospatial
Center under NSF OPP agreement ANT-1043681. Careful reviews by Jeremy
Bassis and two anonymous reviewers significantly improved the
manuscript.
NR 41
TC 18
Z9 18
U1 2
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 29
PY 2012
VL 39
AR L16504
DI 10.1029/2012GL052413
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 999JZ
UT WOS:000308308800001
ER
PT J
AU Vieira, LEA
Norton, A
de Wit, TD
Kretzschmar, M
Schmidt, GA
Cheung, MCM
AF Vieira, L. E. A.
Norton, A.
de Wit, T. Dudok
Kretzschmar, M.
Schmidt, G. A.
Cheung, M. C. M.
TI How the inclination of Earth's orbit affects incoming solar irradiance
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SUN-LIKE STARS; CLIMATE; RECONSTRUCTION; SIMULATIONS; DEPENDENCE;
PATTERNS; ROTATION; CYCLES; FLOW
AB The variability in solar irradiance, the main external energy source of the Earth's system, must be critically studied in order to place the effects of human-driven climate change into perspective and allow plausible predictions of the evolution of climate. Accurate measurements of total solar irradiance (TSI) variability by instruments onboard space platforms during the last three solar cycles indicate changes of approximately 0.1% over the sunspot cycle. Physics-based models also suggest variations of the same magnitude on centennial to millennia time-scales. Additionally, long-term changes in Earth's orbit modulate the solar irradiance reaching the top of the atmosphere. Variations of orbital inclination in relation to the Sun's equator could potentially impact incoming solar irradiance as a result of the anisotropy of the distribution of active regions. Due to a lack of quantitative estimates, this effect has never been assessed. Here, we show that although observers with different orbital inclinations experience various levels of irradiance, modulations in TSI are not sufficient to drive observed 100 kyr climate variations. Based on our model we find that, due to orbital inclination alone, the maximum change in the average TSI over timescales of kyrs is similar to 0.003 Wm(-2), much smaller than the similar to 1.5 Wm(-2) annually integrated change related to orbital eccentricity variations, or the 1-8 Wm(-2) variability due to solar magnetic activity. Here, we stress that out-of-ecliptic measurements are needed in order to constrain models for the long-term evolution of TSI and its impact on climate. Citation: Vieira, L. E. A., A. Norton, T. Dudok de Wit, M. Kretzschmar, G. A. Schmidt, and M. C. M. Cheung (2012), How the inclination of Earth's orbit affects incoming solar irradiance, Geophys. Res. Lett., 39, L16104, doi:10.1029/2012GL052950.
C1 [Vieira, L. E. A.; de Wit, T. Dudok; Kretzschmar, M.] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, UMR7328, FR-45071 Orleans 2, France.
[Norton, A.] Stanford Univ, HEPL, Stanford, CA 94305 USA.
[Kretzschmar, M.] Royal Observ Belgium, SIDC, Brussels, Belgium.
[Schmidt, G. A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Cheung, M. C. M.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA USA.
RP Vieira, LEA (reprint author), Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, UMR7328, 3A,Av Rech, FR-45071 Orleans 2, France.
EM luis.vieira@cnrs-orleans.fr
RI Schmidt, Gavin/D-4427-2012; Vieira, Luis Eduardo/A-5548-2008
OI Schmidt, Gavin/0000-0002-2258-0486; Vieira, Luis
Eduardo/0000-0002-9376-475X
FU European Commission's Seventh Framework Programme (FP7) [261948]
FX We thank the SORCE and SOHO scientific teams for total solar irradiance
data and the Joint Science Operations - Science Data Processing (SDP)
for SDO/HMI images. The TIM/SORCE data is available at
http://lasp.colorado.edu/sorce/data/tsi_data.htm, while the VIRGO/SOHO
data is available at
http://www.pmodwrc.ch/pmod.php?topic=tsi/virgo/proj_space_virgo#Data.
Our work was supported by the European Commission's Seventh Framework
Programme (FP7/2007-2013) under grant agreement 261948 (ATMOP Project).
NR 39
TC 5
Z9 5
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 29
PY 2012
VL 39
AR L16104
DI 10.1029/2012GL052950
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 999JZ
UT WOS:000308308800007
ER
PT J
AU Sun, MG
Cess, RD
Doelling, DR
AF Sun, Moguo
Cess, Robert D.
Doelling, Dave R.
TI Interpretation of cloud structure anomalies over the tropical Pacific
during the 1997/98 El Nino
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; ENERGY SYSTEM CERES; STATISTICAL-ANALYSES;
CLIMATE FEEDBACKS; OBJECT DATA; SATELLITE; PARAMETERIZATION;
TEMPERATURE; VALIDATION; ECMWF
AB Cloud structure changes and their associated radiative property changes over the tropical Pacific Ocean during the strong 1997/98 El Nino are studied using a merged satellite data set from the Clouds and the Earth's Radiant Energy System (CERES) project. This one-degree by one-degree gridded data set provides monthly mean values of radiative fluxes at the top of the atmosphere in addition to cloud fraction, cloud top altitude and cloud optical depth for the first eight months of 1998. This time period includes much of the 1997/98 El Nino, which reached peak intensity in March 1998 and essentially subsided by August 1998. The west-to-east shift of the center of convection that occurred during the El Nino resulted in cloud fraction, cloud top altitude and cloud optical depth increasing in the eastern equatorial Pacific while decreasing in the western tropical Pacific. For both regions all three cloud parameters are strongly correlated with each other and contribute to the strong linear relationship between longwave (LW) and shortwave (SW) cloud-radiative forcings (CRFs). This strong El Nino serves as a suitable test case for climate models. Results using the National Center for Atmospheric Research (NCAR) Community Atmosphere Model (CAM) 4.0 show many of the observed changes in 500 hPa vertical velocity, cloud-radiative forcing, cloud top altitude and cloud fraction within the tropical Pacific during the El Nino event, but fail to capture the observed relationship between radiation anomalies and cloud optical depth anomalies.
C1 [Sun, Moguo] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Cess, Robert D.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
[Doelling, Dave R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Sun, MG (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM moguo.sun@nasa.gov
FU Department of Energy's Office of Science, Biological and Environmental
Research [DEFG0290ER61063, DEFG028ER6013]; NASA CERES Project
FX We thank Minghua Zhang for constructive comments concerning an earlier
draft of this manuscript, in addition to an anonymous reviewer whose
suggestions added considerable clarity to the final paper. This work was
partially supported under the auspices of the Department of Energy's
Office of Science, Biological and Environmental Research through grants
DEFG0290ER61063 and DEFG028ER6013, and by the NASA CERES Project.
NR 30
TC 1
Z9 1
U1 1
U2 6
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 29
PY 2012
VL 117
AR D16114
DI 10.1029/2011JD015861
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 999NI
UT WOS:000308320100001
ER
PT J
AU Hayne, PO
Paige, DA
Schofield, JT
Kass, DM
Kleinbohl, A
Heavens, NG
McCleese, DJ
AF Hayne, Paul O.
Paige, David A.
Schofield, John T.
Kass, David M.
Kleinboehl, Armin
Heavens, Nicholas G.
McCleese, Daniel J.
TI Carbon dioxide snow clouds on Mars: South polar winter observations by
the Mars Climate Sounder
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ORBITER LASER ALTIMETER; MARTIAN SEASONAL CAPS; FROST GRAIN-SIZE;
RADIATIVE-TRANSFER; CO2 ICE; ATMOSPHERE; SURFACE; APPROXIMATION;
TEMPERATURES; BEHAVIOR
AB We present south polar winter infrared observations from the Mars Climate Sounder (MCS) and test three hypotheses concerning the origins of "cold spots": regions of anomalously low infrared brightness temperatures, which could be due to enrichment in non-condensable gases, low-emissivity surface frost, or optically thick CO2 clouds. Clouds and surface frosts have been historically difficult to distinguish, but the unique limb sounding capability of MCS reveals extensive tropospheric CO2 clouds over the cold spots. We find that both clouds and surface deposits play a significant role in lowering the infrared emissivity of the seasonal ice cap, and the granular surface deposits are likely emplaced by snowfall. Surface temperatures indicate the polar winter atmosphere is enriched by a factor similar to 5-7 in non-condensable gases relative to the annual average, consistent with earlier gamma ray spectrometer observations, but not enough to account for the low brightness temperatures. A large similar to 500-km diameter cloud with visible optical depth similar to 0.1-1.0 persists throughout winter over the south polar residual cap (SPRC). At latitudes 70-80 degrees S, clouds and low emission regions are smaller and shorter-lived, probably corresponding to large-grained "channel 1" clouds observed by the Mars Orbiter Laser Altimeter. Snowfall over the SPRC imparts the lowest emissivity in the south polar region, which paradoxically tends to reduce net accumulation of seasonal CO2 by backscattering infrared radiation. This could be compensated by the observed anomalously high summertime albedo of the SPRC, which may be related to small grains preserved in a rapidly formed snow deposit.
C1 [Hayne, Paul O.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hayne, Paul O.; Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Schofield, John T.; Kass, David M.; Kleinboehl, Armin; McCleese, Daniel J.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
[Heavens, Nicholas G.] Cornell Univ, Ithaca, NY USA.
RP Hayne, PO (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM phayne@gps.caltech.edu
OI Heavens, Nicholas/0000-0001-7654-503X
FU National Aeronautics and Space Administration
FX We thank Oded Aharonson, James H. Shirley, and Jennifer L. Benson for
useful discussions and advice during the preparation of this manuscript.
P.O.H. wishes to acknowledge the invaluable support and criticism of the
members of his dissertation committee at UCLA: David A. Paige, Gerald
Schubert, K. N. Liou, and Christopher Russell. Part of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 64
TC 20
Z9 20
U1 1
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD AUG 29
PY 2012
VL 117
AR E08014
DI 10.1029/2011JE004040
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 999NY
UT WOS:000308322000001
ER
PT J
AU Balikhin, MA
Sibeck, DG
Runov, A
Walker, SN
AF Balikhin, M. A.
Sibeck, D. G.
Runov, A.
Walker, S. N.
TI Magnetic holes in the vicinity of dipolarization fronts: Mirror or
tearing structures?
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LOW-FREQUENCY FLUCTUATIONS; INSTABILITY; MAGNETOSHEATH; PLASMAS;
MAGNETOPAUSE; WAVES
AB Magnetic holes filled with isotropic energetic electrons (up to a few 10(5) eV) have been observed by THEMIS in the vicinity of dipolarization fronts. These structures can partially contribute to the initial seed population of energetic electrons within the magnetosphere; therefore finding their nature is important for understanding of the population of high energy electrons within the magnetosphere. Previously, these structures have been interpreted as the result of the mirror instability due to the similarity in their appearance with mirror dips observed in the terrestrial magnetosheath and solar wind. The THEMIS data shown here prove that the measured properties of these structures contradict to the interpretation as mirror waves. In the present study it is shown that these waves do not exhibit the effects on the ion population that are expected due to mirror wave structures. However, they do have a pronounced effect on the high energy electron population. The evolution of the high energy electron population within these structures is investigated. It is then argued that the tearing instability can be responsible for their generation.
C1 [Balikhin, M. A.; Walker, S. N.] Univ Sheffield, ACSE, Dept Automat Control & Syst Engn, Sheffield S1 3JD, S Yorkshire, England.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Runov, A.] Univ Calif Los Angeles, Los Angeles, CA USA.
RP Balikhin, MA (reprint author), Univ Sheffield, ACSE, Dept Automat Control & Syst Engn, Mappin St, Sheffield S1 3JD, S Yorkshire, England.
EM m.balikhin@sheffield.ac.uk
FU ISSI; STFC
FX The authors wish to thank the THEMIS team for providing the observations
reported in this paper. M. A. B. acknowledges support from ISSI and
STFC. The authors are grateful for useful discussions with R. Z.
Sagdeev, A. Artemiev, O. A. Pokhotelov, M. Kuznetsova, and M. Hesse.
NR 33
TC 12
Z9 12
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 29
PY 2012
VL 117
AR A08229
DI 10.1029/2012JA017552
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 999JO
UT WOS:000308307600004
ER
PT J
AU Hwang, KJ
Goldstein, ML
Kuznetsova, MM
Wang, Y
Vinas, AF
Sibeck, DG
AF Hwang, K. -J.
Goldstein, M. L.
Kuznetsova, M. M.
Wang, Y.
Vinas, A. F.
Sibeck, D. G.
TI The first in situ observation of Kelvin-Helmholtz waves at high-latitude
magnetopause during strongly dawnward interplanetary magnetic field
conditions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND CONDITIONS; MAGNETOTAIL BOUNDARY; CLUSTER OBSERVATIONS;
GEOTAIL OBSERVATIONS; EARTHS MAGNETOPAUSE; INSTABILITY; RECONNECTION;
DEPENDENCE; FLOW; MAGNETOSHEATH
AB We report the first in situ observation of high-latitude magnetopause (near the northern duskward cusp) Kelvin-Helmholtz waves (KHW) by Cluster on January 12, 2003, under strongly dawnward interplanetary magnetic field (IMF) conditions. The fluctuations unstable to Kelvin-Helmholtz instability (KHI) are found to propagate mostly tailward, i.e., along the direction almost 90 degrees to both the magnetosheath and geomagnetic fields, which lowers the threshold of the KHI. The magnetic configuration across the boundary layer near the northern duskward cusp region during dawnward IMF is similar to that in the low-latitude boundary layer under northward IMF, in that (1) both magnetosheath and magnetospheric fields across the local boundary layer constitute the lowest magnetic shear and (2) the tailward propagation of the KHW is perpendicular to both fields. Approximately 3-hour-long periods of the KHW during dawnward IMF are followed by the rapid expansion of the dayside magnetosphere associated with the passage of an IMF discontinuity that characterizes an abrupt change in IMF cone angle, phi = acos (B-x/|B|), from similar to 90 degrees to similar to 10 degrees. Cluster, which was on its outbound trajectory, continued observing the boundary waves at the northern evening-side magnetopause during sunward IMF conditions following the passage of the IMF discontinuity. By comparing the signatures of boundary fluctuations before and after the IMF discontinuity, we report that the frequencies of the most unstable KH modes increased after the discontinuity passed. This result demonstrates that differences in IMF orientations (especially in phi) are associated with the properties of KHW at the high-latitude magnetopause due to variations in thickness of the boundary layer, and/or width of the KH-unstable band on the surface of the dayside magnetopause.
C1 [Hwang, K. -J.; Goldstein, M. L.; Wang, Y.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kuznetsova, M. M.; Wang, Y.; Sibeck, D. G.] Univ Maryland, Goddard Planetary & Heliophys Inst, Baltimore, MD 21201 USA.
RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
EM kyoung-joo.hwang@nasa.gov
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA; Magnetospheric Multiscale Interdisciplinary Science grant at the
Goddard Space Flight Center; Goddard [67394324/NCC5-494]
FX This study was supported by NASA's Cluster mission, by a Magnetospheric
Multiscale Interdisciplinary Science grant at the Goddard Space Flight
Center, and by Goddard grant 67394324/NCC5-494 to the UMBC/GEST program.
We acknowledge all Cluster instrument teams, including PEACE, CIS, and
FGM staffs and the Cluster Active Archive (http://caa.estec.esa.int/caa)
from which all the processed science-level data were downloaded.
Simulation results have been provided by the Community Coordinated
Modeling Center at Goddard Space Flight Center through their public Runs
on Request system (http://ccmc.gsfc.nasa.gov). We appreciate both
reviewers' helpful comments and suggestions.
NR 52
TC 18
Z9 18
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 29
PY 2012
VL 117
AR A08233
DI 10.1029/2011JA017256
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 999JO
UT WOS:000308307600002
ER
PT J
AU Thejappa, G
MacDowall, RJ
Bergamo, M
AF Thejappa, G.
MacDowall, R. J.
Bergamo, M.
TI In situ detection of strong Langmuir turbulence processes in solar type
III radio bursts
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ELECTRON-PLASMA OSCILLATIONS; WAVE-WAVE INTERACTIONS; INTERPLANETARY
PLASMA; EMISSION MECHANISMS; SPATIAL COLLAPSE; WIND SPACECRAFT; SOURCE
REGIONS; PROPAGATION; SOLITONS; NUCLEATION
AB The high time resolution observations obtained by the WAVES experiment of the STEREO spacecraft in solar type III radio bursts show that Langmuir waves often occur as intense localized wave packets. These wave packets are characterized by short durations of only a few ms and peak intensities, which well exceed the supersonic modulational instability (MI) thresholds. These timescales and peak intensities satisfy the criterion of the solitons collapsed to spatial scales of a few hundred Debye lengths. The spectra of these wave packets consist of primary spectral peaks corresponding to beam-resonant Langmuir waves, two or more sidebands corresponding to down-shifted and up-shifted daughter Langmuir waves, and low frequency enhancements below a few hundred Hz corresponding to daughter ion sound waves. The frequencies and wave numbers of these spectral components satisfy the resonance conditions of the modulational instability (MI). Moreover, the tricoherences, computed using trispectral analysis techniques show that these spectral components are coupled to each other with a high degree of coherency as expected of the MI type of four wave interactions. The high intensities, short scale lengths, sideband spectral structures and low frequency spectral enhancements and, high levels of tricoherences amongst the spectral components of these wave packets provide unambiguous evidence for the supersonic MI and related strong turbulence processes in type III radio bursts. The implication of these observations include: (1) the MI and related strong turbulence processes often occur in type III source regions, (2) the strong turbulence processes probably play very important roles in beam stabilization as well as conversion of Langmuir waves into escaping radiation at the fundamental and second harmonic of the electron plasma frequency, f(pe), and (3) the Langmuir collapse probably follows the route of MI in type III radio bursts.
C1 [Thejappa, G.; Bergamo, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thejappa, G (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM thejappa.golla@nasa.gov
RI MacDowall, Robert/D-2773-2012
FU NASA [NNX08AO02G, NNX09AB19G, NNX12AH47G]
FX The research of T. G. is supported by the NASA Grants NNX08AO02G,
NNX09AB19G and NNX12AH47G. The SWAVES instruments include contributions
from the Observatoire of Paris, University of Minnesota, University of
California, Berkeley, and NASA/GSFC. We thank the referees for
constructive comments and helpful suggestions.
NR 86
TC 11
Z9 11
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 29
PY 2012
VL 117
AR A08111
DI 10.1029/2012JA017695
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 999JO
UT WOS:000308307600006
ER
PT J
AU Cook, BI
Anchukaitis, KJ
Kaplan, JO
Puma, MJ
Kelley, M
Gueyffier, D
AF Cook, B. I.
Anchukaitis, K. J.
Kaplan, J. O.
Puma, M. J.
Kelley, M.
Gueyffier, D.
TI Pre-Columbian deforestation as an amplifier of drought in Mesoamerica
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID CLASSIC MAYA CIVILIZATION; CLIMATE-CHANGE; COLLAPSE; LOWLANDS; AMERICA;
MEXICO; VARIABILITY; DISTURBANCE; VEGETATION
AB Droughts in pre-Columbian Mesoamerica caused significant societal disruptions during the Late Classic and Post-Classic Periods. While the primary causes of these droughts are still debated, it has been speculated that they may be linked to extensive deforestation associated with high population densities during these intervals. Here we show that pre-Columbian deforestation would have biased the climate in Mesoamerica towards a drier mean state, amplifying drought in the region. In climate model simulations using a pre-Columbian land cover reconstruction, annual precipitation decreases by 5%-15% throughout southern Mexico and the Yucatan compared to simulations using either natural forest cover or forest regrowth associated with population declines after 1500 C. E. These changes are driven primarily by large reductions (10%-20%) in precipitation during the late summer wet season (August-September). When compared to precipitation changes estimated to have occurred during the Maya collapse, our results suggest that deforestation could account for up to sixty percent of the mean drying during this interval. Many regions previously deforested in the pre-Columbian era are now under dense forest cover, indicating potential future climate impacts should tropical deforestation of these areas accelerate. Citation: Cook, B. I., K. J. Anchukaitis, J. O. Kaplan, M. J. Puma, M. Kelley, and D. Gueyffier (2012), Pre-Columbian deforestation as an amplifier of drought in Mesoamerica, Geophys. Res. Lett., 39, L16706, doi:10.1029/2012GL052565.
C1 [Cook, B. I.; Puma, M. J.; Kelley, M.] NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Cook, B. I.; Anchukaitis, K. J.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Kaplan, J. O.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Gueyffier, D.] Off Natl Etud & Rech Aerosp, F-91761 Palaiseau, France.
RP Cook, BI (reprint author), NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM benjamin.i.cook@nasa.gov
RI Cook, Benjamin/H-2265-2012; Gueyffier, Denis/I-4265-2014; Kaplan,
Jed/P-1796-2015;
OI Gueyffier, Denis/0000-0002-4759-3857; Kaplan, Jed/0000-0001-9919-7613;
Anchukaitis, Kevin/0000-0002-8509-8080
FU Swiss National Science Foundation [PP0022_119049]; FIRB [RBID08LNFJ]
FX The authors thanks 2 anonymous reviewers and the editor for providing
comments that greatly improved the quality of this paper. Lamont
Contribution #7563. JOK was supported by Swiss National Science
Foundation professorship grant (PP0022_119049) and FIRB project CASTANEA
(RBID08LNFJ).
NR 36
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U1 1
U2 36
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 25
PY 2012
VL 39
AR L16706
DI 10.1029/2012GL052565
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 995JM
UT WOS:000308004300003
ER
PT J
AU Israelevich, P
Ofman, L
AF Israelevich, P.
Ofman, L.
TI Hybrid simulation of the shock wave trailing the Moon
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND INTERACTION; LUNAR WAKE; LABORATORY SIMULATION; FIELD
STRUCTURE; EXPLORER 35; PLASMA; AU
AB A standing shock wave behind the Moon was predicted by Michel (1967) but never observed nor simulated. We use 1D hybrid code in order to simulate the collapse of the plasma-free cavity behind the Moon and for the first time to model the formation of this shock. Starting immediately downstream of the obstacle we consider the evolution of plasma expansion into the cavity in the frame of reference moving along with the solar wind. Well-known effects as electric charging of the cavity affecting the plasma flow and counterstreaming ion beams in the wake are reproduced. Near the apex of the inner Mach cone where the plasma flows from the opposite sides of the obstacle meet, a shock wave arises. We expect the shock to be produced at periods of high electron temperature solar wind streams (Ti << T-e similar to 100 eV). The shock is produced by the interaction of oppositely directed proton beams in the plane containing solar wind velocity and interplanetary magnetic field vectors. In the direction across the magnetic field and the solar wind velocity, the shock results from the interaction of the plasma flow with the region of the enhanced magnetic field inside the cavity that plays the role of the magnetic barrier. The appearance of the standing shock wave is expected at the distance of similar to 7R(M) downstream of the Moon.
C1 [Israelevich, P.; Ofman, L.] Tel Aviv Univ, Dept Geophys & Planetary Sci, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Ramat Aviv, Israel.
[Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ofman, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Israelevich, P (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Ramat Aviv, Israel.
EM peter@post.tau.ac.il
FU NASA [NNX10AC56G]
FX LO would like to acknowledge support by NASA grant NNX10AC56G.
NR 35
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U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 25
PY 2012
VL 117
AR A08223
DI 10.1029/2011JA017358
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 995KB
UT WOS:000308005800001
ER
PT J
AU Tsuno, K
Dasgupta, R
Danielson, L
Righter, K
AF Tsuno, Kyusei
Dasgupta, Rajdeep
Danielson, Lisa
Righter, Kevin
TI Flux of carbonate melt from deeply subducted pelitic sediments:
Geophysical and geochemical implications for the source of Central
American volcanic arc
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OCEAN ISLAND BASALTS; 3 GPA; METAMORPHIC DEVOLATILIZATION;
HIGH-PRESSURE; MANTLE WEDGE; COSTA-RICA; ECLOGITE; NICARAGUA; VOLATILES;
SILICATE
AB We determined the fluid-present and fluid-absent near-solidus melting of an Al-poor carbonated pelite at 3-7 GPa, to constrain the possible influence of sediment melt in subduction zones. Hydrous silicate melt is produced at the solidi at 3-4 GPa whereas Na-K-rich carbonatite is produced at the solidi at >= 5 GPa for both starting compositions. At >= 5 GPa and 1050 degrees C, immiscible carbonate and silicate melts appear with carbonate melt forming isolated pockets embedded in silicate melt. Application of our data to Nicaraguan slab suggests that sediment melting may not occur at sub-arc depth (similar to 170 km) but carbonatite production can occur atop slab or by diapiric rise of carbonated-silicate melange zone to the mantle wedge at similar to 200-250 km depth. Flux of carbonatite to shallower arc-source can explain the geochemistry of Nicaraguan primary magma (low SiO2 and high CaO, Ba/La). Comparison of carbonate-silicate melt immiscibility field with mantle wedge thermal structure suggests that carbonatite might temporally be trapped in viscous silicate melt, and contribute to seismic low-velocity zone at deep mantle wedge of Nicaragua. Citation: Tsuno, K., R. Dasgupta, L. Danielson, and K. Righter (2012), Flux of carbonate melt from deeply subducted pelitic sediments: Geophysical and geochemical implications for the source of Central American volcanic arc, Geophys. Res. Lett., 39, L16307, doi: 10.1029/2012GL052606.
C1 [Tsuno, Kyusei; Dasgupta, Rajdeep] Rice Univ, Dept Earth Sci, Houston, TX 77005 USA.
[Danielson, Lisa] ESCG, Houston, TX USA.
[Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Tsuno, K (reprint author), Rice Univ, Dept Earth Sci, 6100 Main St,MS 126, Houston, TX 77005 USA.
EM kyusei.tsuno@rice.edu
RI Dasgupta, Rajdeep/C-7252-2009
OI Dasgupta, Rajdeep/0000-0001-5392-415X
FU NSF [OCE-0841035]
FX We thank Anne Peslier and Kent Ross for help with the electron microbe
analyses and greatly appreciate thoughtful comments by two anonymous
reviewers. This work was supported by NSF grant OCE-0841035 to R. D.
NR 37
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U1 3
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 AUG 24
PY 2012
VL 39
AR L16307
DI 10.1029/2012GL052606
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 995JK
UT WOS:000308004100002
ER
PT J
AU Gehrels, N
Meszaros, P
AF Gehrels, Neil
Meszaros, Peter
TI Gamma-Ray Bursts
SO SCIENCE
LA English
DT Review
ID SHORT GRB 090510; STAR-FORMATION HISTORY; HIGH-ENERGY EMISSION; 28
FEBRUARY 1997; FERMI OBSERVATIONS; TELESCOPE OBSERVATIONS; SPECTRAL
COMPONENT; GALAXY EVOLUTION; HOST GALAXY; SWIFT ERA
AB Gamma-ray bursts (GRBs) are bright flashes of gamma rays coming from the cosmos. They occur roughly once per day, typically last for tens of seconds, and are the most luminous events in the universe. More than three decades after their discovery, and after pioneering advances from space and ground experiments, they still remain mysterious. The launch of the Swift and Fermi satellites in 2004 and 2008 brought in a trove of qualitatively new data. In this Review, we survey the interplay between these recent observations and the theoretical models of the prompt GRB emission and the subsequent afterglow.
C1 [Gehrels, Neil] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Gehrels, N (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM neil.gehrels@nasa.gov
NR 68
TC 27
Z9 27
U1 0
U2 2
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 24
PY 2012
VL 337
IS 6097
BP 932
EP 936
DI 10.1126/science.1216793
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 992VI
UT WOS:000307807600036
PM 22923573
ER
PT J
AU Reis, RC
Miller, JM
Reynolds, MT
Gultekin, K
Maitra, D
King, AL
Strohmayer, TE
AF Reis, R. C.
Miller, J. M.
Reynolds, M. T.
Gueltekin, K.
Maitra, D.
King, A. L.
Strohmayer, T. E.
TI A 200-Second Quasi-Periodicity After the Tidal Disruption of a Star by a
Dormant Black Hole
SO SCIENCE
LA English
DT Article
ID X-RAY BINARIES; ACTIVE GALACTIC NUCLEI; SWIFT J164449.3+573451;
FUNDAMENTAL PLANE; ACCRETION FLOWS; OSCILLATION; DISCOVERY; OUTBURST;
GALAXY; MASS
AB Supermassive black holes (SMBHs; mass is greater than or approximately 10(5) times that of the Sun) are known to exist at the center of most galaxies with sufficient stellar mass. In the local universe, it is possible to infer their properties from the surrounding stars or gas. However, at high redshifts we require active, continuous accretion to infer the presence of the SMBHs, which often comes in the form of long-term accretion in active galactic nuclei. SMBHs can also capture and tidally disrupt stars orbiting nearby, resulting in bright flares from otherwise quiescent black holes. Here, we report on a similar to 200-second x-ray quasi-periodicity around a previously dormant SMBH located in the center of a galaxy at redshift z = 0.3534. This result may open the possibility of probing general relativity beyond our local universe.
C1 [Reis, R. C.; Miller, J. M.; Reynolds, M. T.; Gueltekin, K.; Maitra, D.; King, A. L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Strohmayer, T. E.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Reis, RC (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
EM rdosreis@umich.edu
OI reis, rubens/0000-0002-6618-2412; Gultekin, Kayhan/0000-0002-1146-0198
FU Michigan Society of Fellows; NASA [PF1-120087]; ESA; United States
(NASA); Suzaku satellite; Japan (Japan Aerospace Exploration Agency)
FX R.C.R. thanks the Michigan Society of Fellows and NASA for support
through the Einstein Fellowship Program, grant PF1-120087. R. C. R. also
thanks C. Reynolds and R. Mushotzky for comments on our early work. We
all thank N. Schartel and the XMM-Newton staff for executing monitoring
observations of Swift J164449.3+573451. This work is based on
observations made with XMM-Newton, a European Space Agency (ESA) science
mission with instruments and contributions directly funded by ESA member
states and the United States (NASA), and the Suzaku satellite, a
collaborative mission between the space agencies of Japan (Japan
Aerospace Exploration Agency) and the USA (NASA). This work also made
use of data supplied by the UK Swift Science Data Centre at the
University of Leicester.
NR 34
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U1 1
U2 7
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 24
PY 2012
VL 337
IS 6097
BP 949
EP 951
DI 10.1126/science.1223940
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 992VI
UT WOS:000307807600040
PM 22859817
ER
PT J
AU Eastwood, JP
Phan, TD
Fear, RC
Sibeck, DG
Angelopoulos, V
Oieroset, M
Shay, MA
AF Eastwood, J. P.
Phan, T. D.
Fear, R. C.
Sibeck, D. G.
Angelopoulos, V.
Oieroset, M.
Shay, M. A.
TI Survival of flux transfer event (FTE) flux ropes far along the tail
magnetopause
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; EARTHS MAGNETOPAUSE; PLASMA ENTRY;
SOLAR-WIND; RECONNECTION; DEPENDENCE; IMF; CLOUDS; REGION; TIME
AB During intervals of southward IMF, magnetic reconnection can result in the formation of flux transfer events (FTEs) on the dayside magnetopause which travel along the magnetopause in the anti-sunward direction. Of particular interest is their fate and the role they play transporting solar wind plasma into the magnetosphere. We present the discovery of FTEs far along the distant tail magnetopause (x = -67 Earth radii) using data from ARTEMIS on the dusk flank magnetopause under southward/duskward IMF conditions. The identification of several events is further supported by excellent fits to a force-free flux rope model. The axis of each structure is principally north-south, i.e., perpendicular to the Sun-Earth line. Simultaneous observations by THEMIS on the dayside magnetopause indicate that FTEs are being produced there, although perhaps 2-4 times smaller in size. The convection time from the dayside magnetopause to ARTEMIS is 30 min, and the FTEs have a flux content comparable to those typically observed on the dayside magnetopause, indicating that these features are in quasi-equilibrium as they are convected downtail. By considering the relative orientations of the FTEs observed by THEMIS and ARTEMIS, the magnetic field geometry is consistent with the FTEs being produced on the dayside magnetopause along an extended X-line in the presence of IMF B-y and bending as they are convected to the flanks.
C1 [Eastwood, J. P.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Phan, T. D.; Oieroset, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Fear, R. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Shay, M. A.] Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA.
RP Eastwood, JP (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England.
EM jonathan.eastwood@imperial.ac.uk
RI Shay, Michael/G-5476-2013; NASA MMS, Science Team/J-5393-2013;
OI NASA MMS, Science Team/0000-0002-9504-5214; Fear,
Robert/0000-0003-0589-7147
FU STFC at ICL; NASA [NAS5-02099]; German Ministry for Economy and
Technology; German Center for Aviation and Space (DLR) [50 OC 0302]
FX J.P.E. holds an STFC Advanced Fellowship at ICL. We acknowledge NASA
contract NAS5-02099 for use of data from the THEMIS Mission,
specifically D. Larson and R. P. Lin for use of SST data; C. W. Carlson
and J. P. McFadden for use of ESA data; and K. H. Glassmeier, U. Auster,
and W. Baumjohann for the use of FGM data provided under the lead of the
Technical University of Braunschweig and with financial support through
the German Ministry for Economy and Technology and the German Center for
Aviation and Space (DLR) under contract 50 OC 0302.
NR 44
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U1 2
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 23
PY 2012
VL 117
AR A08222
DI 10.1029/2012JA017722
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 995JX
UT WOS:000308005400004
ER
PT J
AU Tsurutani, BT
Falkowski, BJ
Verkhoglyadova, OP
Pickett, JS
Santolik, O
Lakhina, GS
AF Tsurutani, Bruce T.
Falkowski, Barbara J.
Verkhoglyadova, Olga P.
Pickett, Jolene S.
Santolik, Ondrej
Lakhina, Gurbax S.
TI Dayside ELF electromagnetic wave survey: A Polar statistical study of
chorus and hiss
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID WHISTLER-MODE CHORUS; VLF LINE RADIATION; PLASMASPHERIC HISS; EQUATORIAL
NOISE; MAGNETOSONIC WAVES; PROPAGATION CHARACTERISTICS; MAGNETIC
EQUATOR; EMISSIONS; MAGNETOSPHERE; PLASMAPAUSE
AB Statistical analyses of Polar plasma wave data are performed to determine the occurrence frequency, intensity, and Poynting direction of similar to 360 Hz to similar to 1.8 kHz extremely low-frequency (ELF) electromagnetic waves (chorus, magnetosonic mode, and hiss) in the dayside sector of the magnetosphere. The study is limited to an L* range of 2 to 9 and a magnetic local time (MLT) range of 0900 to 1500, a region infrequently covered in past statistical surveys. The study was performed on 1996-1997 data, an interval near solar minimum. It is determined that in the outer region of the magnetosphere, from L* = 6 to 9, the similar to 360 to similar to 800 Hz waves at Polar altitudes are typically characterized by downward (toward Earth) propagation. The downgoing waves have been previously identified as chorus in Tsurutani et al. (2011). The downgoing chorus have intensities of similar to 10(-2) nT(2), are right-hand circularly polarized and are propagating close to parallel to the ambient magnetic field B-0. The high rate of occurrence of these downward propagating waves narrows to a smaller region of L* = 6 to 7 for similar to 1.2 kHz waves. In the inner region of the magnetosphere, L* = 3 to 6, the similar to 360 to 800 Hz waves are characteristically oblique (to B0) and upwards propagating, away from the Earth. The upcoming waves are most likely plasmaspheric hiss and low altitude magnetospherically reflected waves. These waves are an order of magnitude less intense and less coherent than the downward propagating chorus waves. At low frequencies, similar to 360 Hz, there is a region near L* = 4 to 5, where obliquely propagating waves are detected. These are most probably a mixture of obliquely propagating plasmaspheric hiss and magnetosonic waves. A detailed (case study) examination of upward propagating waves is made for one Polar pass to add context to the statistical results. The upward propagating waves are quasicoherent and slightly elliptically polarized at Polar altitudes. From this and the statistical results, we ascribe to the scenario that similar to 360 to 800 Hz chorus enters the plasmasphere at low altitude entry points and propagates through the plasmasphere as semicoherent hiss, in basic agreement with the Bortnik et al. (2008, 2009a) hypothesis for the origin of some plasmaspheric hiss. However, for similar to 1.2 and 1.8 kHz waves inside the nominal location of the plasmasphere, downward propagating waves have higher intensities than upward propagating or oblique waves, perhaps indicating effects associated with different source locations, different entry points and different reflection regions and/or damping/amplification. At similar to 800 Hz and similar to 1.2 kHz upward propagating waves with weak intensities are common in the range L* = 8-9. These may be chorus waves magnetospherically reflected to larger L*. For frequencies above similar to 1.5 kHz, most wave events are low intensity and upward propagating. It is possible that sferics and power line harmonics are contributors to these signals.
C1 [Tsurutani, Bruce T.; Falkowski, Barbara J.; Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Falkowski, Barbara J.] Glendale City Coll, Dept Phys, Glendale, CA USA.
[Falkowski, Barbara J.] Glendale City Coll, Dept Astron, Glendale, CA USA.
[Verkhoglyadova, Olga P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Pickett, Jolene S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Santolik, Ondrej] Inst Atmospher Phys, Prague, Czech Republic.
[Santolik, Ondrej] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.
[Lakhina, Gurbax S.] Indian Inst Geomagnetism, Navi Mumbai, India.
RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bruce.t.tsurutani@jpl.nasa.gov
RI Santolik, Ondrej/F-7766-2014;
OI Lakhina, Gurbax /0000-0002-8956-486X; Verkhoglyadova,
Olga/0000-0002-9295-9539
FU NASA; Indian National Science Academy, New Delhi; JPL [1246597]; [GACR
105/10/2279]; [ME10001]
FX Portions of this work were performed at the Jet Propulsion Laboratory,
California Institute of Technology under contract with NASA. GSL thanks
the Indian National Science Academy, New Delhi, for support under the
Senior Scientist Scheme. JSP and OS acknowledge JPL support under
Subcontract 1246597. OS acknowledges additional support from grants GACR
105/10/2279 and ME10001. We acknowledge critical comments given by E.
Echer, who helped us discuss interplanetary drivers, and D. Galvan and
J. Goldstein for plasmaspheric dynamics, respectively. We thank the two
referees for their critical and constructive comments which have helped
improve this work.
NR 107
TC 16
Z9 16
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 23
PY 2012
VL 117
AR A00L12
DI 10.1029/2011JA017180
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 995JX
UT WOS:000308005400001
ER
PT J
AU Simpson, IJ
Andersen, MPS
Meinardi, S
Bruhwiler, L
Blake, NJ
Helmig, D
Rowland, FS
Blake, DR
AF Simpson, Isobel J.
Andersen, Mads P. Sulbaek
Meinardi, Simone
Bruhwiler, Lori
Blake, Nicola J.
Helmig, Detlev
Rowland, F. Sherwood
Blake, Donald R.
TI Long-term decline of global atmospheric ethane concentrations and
implications for methane
SO NATURE
LA English
DT Article
ID EMISSIONS; VARIABILITY; BUDGET; GASES; MODEL
AB After methane, ethane is the most abundant hydrocarbon in the remote atmosphere. It is a precursor to tropospheric ozone and it influences the atmosphere's oxidative capacity through its reaction with the hydroxyl radical, ethane's primary atmospheric sink(1-3). Here we present the longest continuous record of global atmospheric ethane levels. We show that global ethane emission rates decreased from 14.3 to 11.3 teragrams per year, or by 21 per cent, from 1984 to 2010. We attribute this to decreasing fugitive emissions from ethane's fossil fuel source-most probably decreased venting and flaring of natural gas in oil fields-rather than a decline in its other major sources, biofuel use and biomass burning. Ethane's major emission sources are shared with methane, and recent studies have disagreed on whether reduced fossil fuel or microbial emissions have caused methane's atmospheric growth rate to slow(4,5). Our findings suggest that reduced fugitive fossil fuel emissions account for at least 10-21 teragrams per year (30-70 per cent) of the decrease in methane's global emissions, significantly contributing to methane's slowing atmospheric growth rate since the mid-1980s.
C1 [Simpson, Isobel J.; Andersen, Mads P. Sulbaek; Meinardi, Simone; Blake, Nicola J.; Rowland, F. Sherwood; Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA.
[Andersen, Mads P. Sulbaek] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bruhwiler, Lori] NOAA, ESRL, Boulder, CO 80305 USA.
[Helmig, Detlev] Univ Colorado, Inst Arctic & Alpine Res INSTAAR, Boulder, CO 80309 USA.
RP Simpson, IJ (reprint author), Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA.
EM isimpson@uci.edu
RI Sulbaek Andersen, Mads/C-4708-2008
OI Sulbaek Andersen, Mads/0000-0002-7976-5852
FU NASA [NAG5-8935]; Gary Comer Abrupt Climate Change Fellowship
FX This research was funded by NASA (grant NAG5-8935), with contributions
from the Gary Comer Abrupt Climate Change Fellowship. We acknowledge
discussions with many colleagues, especially M. Aydin and C. Wiedinmyer.
We thank colleagues at the Norfolk Island Bureau of Meteorology and the
NOAA research stations in Samoa and Barrow for sample collection; the
UCI team for sample collection and analysis, especially B. Chisholm, R.
Day, G. Liu, B. Love and M. McEachern; and K. Masarie for work with the
NOAA/INSTAAR data. M.P.S.A. is supported at JPL by an appointment to the
NASA Postdoctoral Program, administered by Oak Ridge Associated
Universities through a contract with NASA.
NR 30
TC 61
Z9 65
U1 6
U2 112
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD AUG 23
PY 2012
VL 488
IS 7412
BP 490
EP 494
DI 10.1038/nature11342
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 992FS
UT WOS:000307761600032
PM 22914166
ER
PT J
AU Hartle, RE
Johnson, RE
Sittler, EC
Sarantos, M
Simpson, DG
AF Hartle, R. E.
Johnson, R. E.
Sittler, E. C., Jr.
Sarantos, M.
Simpson, D. G.
TI Wind-induced atmospheric escape: Titan
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID PLANETARY EXOSPHERES; SPECTROMETER; ION; DISTRIBUTIONS; NITROGEN;
PLASMA; MODEL
AB Rapid thermospheric flows can significantly enhance the atmospheric loss rates and structures of atmospheric coronae of planetary bodies. Using descriptions of atmospheric escape based on molecular kinetic models, we show that such flows at the exobase of Titan could significantly increase the calculated constituent thermal and nonthermal escape rates. In particular, we show here that the effect of thermospheric winds at the exobase cannot be ignored when calculating the escape of methane from Titan. Such enhancements are likely also relevant to Pluto and exoplanet atmospheres. Citation: Hartle, R.E., R.E. Johnson, E.C. Sittler Jr., M. Sarantos, and D.G. Simpson (2012), Wind-induced atmospheric escape: Titan, Geophys. Res. Lett., 39, L16201, doi: 10.1029/2012GL052774.
C1 [Hartle, R. E.; Sittler, E. C., Jr.; Sarantos, M.; Simpson, D. G.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Hartle, R. E.; Sarantos, M.] NASA, Lunar Sci Inst, Moffett Field, CA USA.
[Johnson, R. E.] Univ Virginia, Charlottesville, VA USA.
[Sarantos, M.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Hartle, RE (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Code 670, Greenbelt, MD 20771 USA.
EM richard.e.hartle@nasa.gov
RI Sarantos, Menelaos/H-8136-2013
FU Cassini Plasma Spectrometer (CAPS) Project through NASA Jet Propulsion
Laboratory contract [1243218]; Southwest Research Institute in San
Antonio, Texas; NASA's Planetary Atmospheres Program
FX This work was supported at NASA Goddard Space Flight Center by the
Cassini Plasma Spectrometer (CAPS) Project through NASA Jet Propulsion
Laboratory contract 1243218 with the Southwest Research Institute in San
Antonio, Texas. REH and MS also acknowledge the Dynamic Response of the
Environment At the Moon (DREAM), NASA Lunar Science Institute. REJ
acknowledges support from NASA's Planetary Atmospheres Program.
NR 30
TC 2
Z9 2
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 AUG 22
PY 2012
VL 39
AR L16201
DI 10.1029/2012GL052774
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 995JG
UT WOS:000308003700002
ER
PT J
AU Tzortziou, M
Herman, JR
Cede, A
Abuhassan, N
AF Tzortziou, Maria
Herman, Jay R.
Cede, Alexander
Abuhassan, Nader
TI High precision, absolute total column ozone measurements from the
Pandora spectrometer system: Comparisons with data from a Brewer double
monochromator and Aura OMI
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPOSPHERIC OZONE; NITROGEN-DIOXIDE; UV MEASUREMENTS; MAX-DOAS;
IRRADIANCE; SPECTROPHOTOMETER; PHOTOCHEMISTRY; ABSORPTION; CABAUW; NO2
AB We present new, high precision, high temporal resolution measurements of total column ozone (TCO) amounts derived from ground-based direct-sun irradiance measurements using our recently deployed Pandora single-grating spectrometers. Pandora's small size and portability allow deployment at multiple sites within an urban air-shed and development of a ground-based monitoring network for studying small-scale atmospheric dynamics, spatial heterogeneities in trace gas distribution, local pollution conditions, photochemical processes and interdependencies of ozone and its major precursors. Results are shown for four mid-to high-latitude sites where different Pandora instruments were used. Comparisons with a well calibrated double-grating Brewer spectrometer over a period of more than a year in Greenbelt MD showed excellent agreement and a small bias of approximately 2 DU (or, 0.6%). This was constant with slant column ozone amount over the full range of observed solar zenith angles (15-80 degrees), indicating adequate Pandora stray light correction. A small (1-2%) seasonal difference was found, consistent with sensitivity studies showing that the Pandora spectral fitting TCO retrieval has a temperature dependence of 1% per 3 degrees K, with an underestimation in temperature (e. g., during summer) resulting in an underestimation of TCO. Pandora agreed well with Aura-OMI (Ozone Measuring Instrument) satellite data, with average residuals of <1% at the different sites when the OMI view was within 50 km from the Pandora location and OMI-measured cloud fraction was <0.2. The frequent and continuous measurements by Pandora revealed significant short-term (hourly) temporal changes in TCO, not possible to capture by sun-synchronous satellites, such as OMI, alone.
C1 [Tzortziou, Maria; Herman, Jay R.; Cede, Alexander; Abuhassan, Nader] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tzortziou, Maria] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Herman, Jay R.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Cede, Alexander] LuftBlick, Kreith, Austria.
[Abuhassan, Nader] Morgan State Univ, Sch Engn, Baltimore, MD 21239 USA.
RP Tzortziou, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM maria.a.tzortziou@nasa.gov
OI Herman, Jay/0000-0002-9146-1632
NR 62
TC 14
Z9 14
U1 0
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 22
PY 2012
VL 117
AR D16303
DI 10.1029/2012JD017814
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 996GA
UT WOS:000308071700004
ER
PT J
AU Clancy, RT
Sandor, BJ
Wolff, MJ
Smith, MD
Lefevre, F
Madeleine, JB
Forget, F
Murchie, SL
Seelos, FP
Seelos, KD
Nair, HA
Toigo, AD
Humm, D
Kass, DM
Kleinbohl, A
Heavens, N
AF Clancy, R. Todd
Sandor, Brad J.
Wolff, Michael J.
Smith, Michael D.
Lefevre, Franck
Madeleine, Jean-Baptiste
Forget, Francois
Murchie, Scott L.
Seelos, Frank P.
Seelos, Kim D.
Nair, Hari A.
Toigo, Anthony D.
Humm, David
Kass, David M.
Kleinboehl, Armin
Heavens, Nicholas
TI Extensive MRO CRISM observations of 1.27 mu m O-2 airglow in Mars polar
night and their comparison to MRO MCS temperature profiles and LMD GCM
simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MARTIAN ATMOSPHERE; 1.27-MU-M; OZONE; RECOMBINATION; CIRCULATION;
EMISSION; APHELION; DAYGLOW; SURFACE; CLOUDS
AB The Martian polar night distribution of 1.27 mu m (0-0) band emission from O-2 singlet delta [O-2((1)Delta(g))] is determined from an extensive set of Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectral Mapping (CRISM) limb scans observed over a wide range of Mars seasons, high latitudes, local times, and longitudes between 2009 and 2011. This polar nightglow reflects meridional transport and winter polar descent of atomic oxygen produced from CO2 photodissociation. A distinct peak in 1.27 mu m nightglow appears prominently over 70-90NS latitudes at 40-60 km altitudes, as retrieved for over 100 vertical profiles of O-2((1)Delta(g)) 1.27 mu m volume emission rates (VER). We also present the first detection of much (x80 +/- 20) weaker 1.58 mu m (0-1) band emission from Mars O-2((1)Delta(g)). Co-located polar night CRISM O-2((1)Delta(g)) and Mars Climate Sounder (MCS) (McCleese et al., 2008) temperature profiles are compared to the same profiles as simulated by the Laboratoire de Meteorologie Dynamique (LMD) general circulation/photochemical model (e. g., Lefevre et al., 2004). Both standard and interactive aerosol LMD simulations (Madeleine et al., 2011a) underproduce CRISM O-2((1)Delta(g)) total emission rates by 40%, due to inadequate transport of atomic oxygen to the winter polar emission regions. Incorporation of interactive cloud radiative forcing on the global circulation leads to distinct but insufficient improvements in modeled polar O-2((1)Delta(g)) and temperatures. The observed and modeled anti-correlations between temperatures and 1.27 mu m band VER reflect the temperature dependence of the rate coefficient for O-2((1)Delta(g)) formation, as provided in Roble (1995).
C1 [Clancy, R. Todd; Sandor, Brad J.; Wolff, Michael J.] Space Sci Inst, Boulder, CO 80301 USA.
[Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lefevre, Franck] Lab Atmospheres Milieux Observat Spatiales, Paris, France.
[Madeleine, Jean-Baptiste; Forget, Francois] Meteorol Dynam Lab, Paris, France.
[Murchie, Scott L.; Seelos, Frank P.; Seelos, Kim D.; Nair, Hari A.; Toigo, Anthony D.; Humm, David] Johns Hopkins Univ, Appl Phys Lab, Columbia, MD USA.
[Kass, David M.; Kleinboehl, Armin; Heavens, Nicholas] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Clancy, RT (reprint author), Space Sci Inst, 4750 Walnut St,Ste 205, Boulder, CO 80301 USA.
EM clancy@spacescience.org
RI Murchie, Scott/E-8030-2015; Seelos, Kimberly/F-4647-2015; Humm,
David/B-8825-2016; Seelos, Frank/C-7875-2016
OI Murchie, Scott/0000-0002-1616-8751; Seelos,
Kimberly/0000-0001-7236-0580; Humm, David/0000-0003-1520-261X; Seelos,
Frank/0000-0001-9721-941X
FU NASA MDAP Program under NASA [NNX10AL61G]
FX We are indebted to the excellent MRO and CRISM operations staff for the
collection and processing of CRISM limb observations presented here.
Grant support for this work was provided by the NASA MDAP Program (under
NASA contract award number NNX10AL61G).
NR 54
TC 10
Z9 10
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD AUG 22
PY 2012
VL 117
AR E00J10
DI 10.1029/2011JE004018
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 995LM
UT WOS:000308009600002
ER
PT J
AU Wintucky, EG
Simons, RN
Freeman, JC
Chevalier, CT
Abraham, AJ
AF Wintucky, E. G.
Simons, R. N.
Freeman, J. C.
Chevalier, C. T.
Abraham, A. J.
TI High-efficiency three-way Ka-band waveguide unequal power combiner
SO IET MICROWAVES ANTENNAS & PROPAGATION
LA English
DT Article
AB This article presents the design, simulation and characterisation of a novel high-efficiency Ka-band (32.05 +/- 0.25 GHz) rectangular waveguide three-way serial combiner for monolithic microwave integrated circuit power amplifiers (PAs) with unequal output power. The combiner presented here is suited for low data rate communications from deep space using a single carrier with constant envelope (amplitude) type modulation. The three-way combiner consists internally of two branch-line hybrids connected in series by a short length of waveguide. The two branch-line hybrids were each designed to combine two input signals that are equal in phase and with an amplitude ratio of two, although in general the amplitude ratio could be arbitrary. The combiner was fabricated in an E-plane split-block arrangement and precision machined from blocks of aluminium with standard WR-28 waveguide ports. S-parameter measurements demonstrated a close achievement of the design goals. The measured return loss at the output port was greater than 16 dB and the isolation between the three input ports of the three-way combiner were greater than 22 dB. The combining of three PAs was successfully demonstrated in which the measured combining efficiency was greater than 90% at the centre frequency of 32.05 GHz.
C1 [Wintucky, E. G.; Simons, R. N.; Freeman, J. C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Chevalier, C. T.] QinetiQ N Amer Corp, Cleveland, OH 44135 USA.
[Abraham, A. J.] Lehigh Univ, Dept Mech Engn, Bethlehem, PA 18015 USA.
RP Wintucky, EG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Edwin.G.Wintucky@nasa.gov
NR 8
TC 3
Z9 4
U1 1
U2 3
PU INST ENGINEERING TECHNOLOGY-IET
PI HERTFORD
PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND
SN 1751-8725
J9 IET MICROW ANTENNA P
JI IET Microw. Antennas Propag.
PD AUG 21
PY 2012
VL 6
IS 11
BP 1195
EP 1199
DI 10.1049/iet-map.2012.0207
PG 5
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 022JE
UT WOS:000309953500001
ER
PT J
AU Cooper, MJ
Martin, RV
van Donkelaar, A
Lamsal, L
Brauer, M
Brook, JR
AF Cooper, Matthew J.
Martin, Randall V.
van Donkelaar, Aaron
Lamsal, Lok
Brauer, Michael
Brook, Jeffrey R.
TI A Satellite-Based Multi-Pollutant Index of Global Air Quality
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Editorial Material
C1 [Cooper, Matthew J.; Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Halifax, NS B3H 3J5, Canada.
[Martin, Randall V.; Brook, Jeffrey R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lamsal, Lok] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Lamsal, Lok] NASA, Atmospher Chem & Dynam Lab, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Brauer, Michael] Univ British Columbia, Vancouver, BC V6T 1Z3, Canada.
[Martin, Randall V.; Brook, Jeffrey R.] Environm Canada, Air Qual Proc Res Sect, Toronto, ON M6B 2S7, Canada.
RP Cooper, MJ (reprint author), Dalhousie Univ, Halifax, NS B3H 3J5, Canada.
EM cooperm2@dal.ca
RI Lamsal, Lok/G-4781-2012; Martin, Randall/C-1205-2014;
OI Martin, Randall/0000-0003-2632-8402; Brauer, Michael/0000-0002-9103-9343
NR 5
TC 9
Z9 9
U1 1
U2 26
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD AUG 21
PY 2012
VL 46
IS 16
BP 8523
EP 8524
DI 10.1021/es302672p
PG 2
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 991JQ
UT WOS:000307697700001
PM 22853810
ER
PT J
AU Kurtz, NT
Markus, T
AF Kurtz, N. T.
Markus, T.
TI Satellite observations of Antarctic sea ice thickness and volume
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SOUTHERN-OCEAN; SNOW DEPTH; EAST ANTARCTICA; VARIABILITY;
BELLINGSHAUSEN; ACCUMULATION; FREEBOARD; AMUNDSEN; COVER; MODEL
AB We utilize satellite laser altimetry data from NASA's Ice, Cloud, and land Elevation Satellite (ICESat) combined with passive microwave measurements to analyze basin-wide changes in Antarctic sea ice thickness and volume over a 5 year period from 2003-2008. Sea ice thickness exhibits a small negative trend while area increases in the summer and fall balanced losses in thickness leading to small overall volume changes. Using a 5 year time series, we show that only small ice thickness changes of less than -0.03 m/yr and volume changes of -266 km(3)/yr and 160 km(3)/yr occurred for the spring and summer periods, respectively. These results are in stark contrast to the much greater observed losses in Arctic sea ice volume and illustrate the different hemispheric changes of the polar sea ice covers in recent years. The uncertainties in the calculated thickness and volume trends are large compared to the observed basin-scale trends. This masks the determination of a long-term trend or cyclical variability in the sea ice cover. It is found that lengthening of the observation time series along with better determination of the interannual variability of sea ice and snow densities will allow for a more statistically significant determination of long-term sea ice thickness and volume trends in the Southern Ocean.
C1 [Kurtz, N. T.] Morgan State Univ, Baltimore, MD 21251 USA.
[Kurtz, N. T.; Markus, T.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
RP Kurtz, NT (reprint author), Morgan State Univ, Baltimore, MD 21251 USA.
EM nathan.t.kurtz@nasa.gov
NR 45
TC 39
Z9 46
U1 2
U2 35
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD AUG 21
PY 2012
VL 117
AR C08025
DI 10.1029/2012JC008141
PG 9
WC Oceanography
SC Oceanography
GA 995QK
UT WOS:000308026500003
ER
PT J
AU Long, MD
Till, CB
Druken, KA
Carlson, RW
Wagner, LS
Fouch, MJ
James, DE
Grove, TL
Schmerr, N
Kincaid, C
AF Long, Maureen D.
Till, Christy B.
Druken, Kelsey A.
Carlson, Richard W.
Wagner, Lara S.
Fouch, Matthew J.
James, David E.
Grove, Timothy L.
Schmerr, Nicholas
Kincaid, Chris
TI Mantle dynamics beneath the Pacific Northwest and the generation of
voluminous back-arc volcanism
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE intraplate volcanism; mantle dynamics; mantle upwelling; slab rollback;
subduction
ID WESTERN UNITED-STATES; TRANSPORTABLE ARRAY DATA; WAVE VELOCITY
STRUCTURE; TRAVEL-TIME TOMOGRAPHY; COLUMBIA RIVER BASALT; HIGH LAVA
PLAINS; YELLOWSTONE HOTSPOT; SUBDUCTION ZONES; FLOOD BASALTS; TECTONIC
ROTATION
AB The Pacific Northwest (PNW) has a complex tectonic history and over the past similar to 17 Ma has played host to several major episodes of intraplate volcanism. These events include the Steens/Columbia River flood basalts (CRB) and the striking spatiotemporal trends of the Yellowstone/Snake River Plain (Y/SRP) and High Lava Plains (HLP) regions. Several different models have been proposed to explain these features, which variously invoke the putative Yellowstone plume, rollback and steepening of the Cascadia slab, extensional processes in the lithosphere, or a combination of these. Here we integrate seismologic, geodynamic, geochemical, and petrologic results from the multidisciplinary HLP project and associated analyses of EarthScope USArray seismic data to propose a conceptual model for post-20 Ma mantle dynamics beneath the PNW and the relationships between mantle flow and surface tectonomagmatic activity. This model invokes rollback subduction as the main driver for mantle flow beneath the PNW beginning at similar to 20 Ma. A major pulse of upwelling due to slab rollback and upper plate extension and consequent melting produced the Steens/CRB volcanism, and continuing trench migration enabled mantle upwelling and hot, shallow melting beneath the HLP. An additional buoyant mantle upwelling is required to explain the Y/SRP volcanism, but subduction-related processes may well have played a primary role in controlling its timing and location, and this upwelling likely continues today in some form. This conceptual model makes predictions that are broadly consistent with seismic observations, geodynamic modeling experiments, and petrologic and geochemical constraints.
C1 [Long, Maureen D.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA.
[Till, Christy B.; Grove, Timothy L.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Druken, Kelsey A.; Kincaid, Chris] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA.
[Druken, Kelsey A.; Carlson, Richard W.; Fouch, Matthew J.; James, David E.; Schmerr, Nicholas] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Wagner, Lara S.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA.
[Schmerr, Nicholas] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Long, MD (reprint author), Yale Univ, Dept Geol & Geophys, POB 208109, New Haven, CT 06520 USA.
EM maureen.long@yale.edu
RI Till, Christy/D-7771-2012; Grove, Timothy/M-9638-2013; Long,
Maureen/A-1383-2009;
OI Grove, Timothy/0000-0003-0628-1969; Long, Maureen/0000-0003-1936-3840;
Schmerr, Nicholas/0000-0002-3256-1262
FU NSF Continental Dynamics program [EAR-0507248, EAR-0506914, EAR-0507486,
EAR-0506857]; NSF EarthScope Science program [EAR-0548288]; NSF
[EAR-0809192]; Alfred P. Sloan Research Fellowship
FX This work is part of the High Lava Plains Project, with support provided
by the NSF Continental Dynamics program through grants EAR-0507248
(MJF), EAR-0506914 (DEJ and RWC), EAR-0507486 (TLG) and EAR-0506857
(CK). MJF acknowledges additional support from the NSF EarthScope
Science program through grant EAR-0548288. LSW's participation was
supported through NSF grant EAR-0809192, and MDL acknowledges support
from an Alfred P. Sloan Research Fellowship. Seismic data from the
USArray Transportable Array network and from the HLP Broadband Seismic
Experiment were used in this study, and we thank the vast network of
people involved in making these experiments a success. We are
particularly grateful to the IRIS PASSCAL and DMC programs for enabling
the collection, archiving, and distribution of TA and HLP broadband
data, and to Jenda Johnson, Steven Golden, the Eastern Oregon
Agricultural Research Center, and the many landowners and field
volunteers who made the HLP deployment possible. Finally, we are
grateful to Claudio Faccenna, Brandon Schmandt, and an anonymous
reviewer for thoughtful and constructive comments that greatly improved
the manuscript.
NR 122
TC 15
Z9 15
U1 4
U2 54
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD AUG 21
PY 2012
VL 13
AR Q0AN01
DI 10.1029/2012GC004189
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 995JR
UT WOS:000308004800002
ER
PT J
AU Li, JLF
Waliser, DE
Chen, WT
Guan, B
Kubar, T
Stephens, G
Ma, HY
Deng, M
Donner, L
Seman, C
Horowitz, L
AF Li, J-L. F.
Waliser, D. E.
Chen, W-T.
Guan, B.
Kubar, T.
Stephens, G.
Ma, H-Y.
Deng, M.
Donner, L.
Seman, C.
Horowitz, L.
TI An observationally based evaluation of cloud ice water in CMIP3 and
CMIP5 GCMs and contemporary reanalyses using contemporary satellite data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; LARGE-SCALE MODELS; PHASE ARCTIC CLOUD;
FRONTAL CLOUDS; SINGLE-COLUMN; GLOBAL PRECIPITATION; TROPICAL
CONVECTION; STRATIFORM CLOUDS; RETRIEVAL METHODS; RESOLVING MODELS
AB We perform an observationally based evaluation of the cloud ice water content (CIWC) and path (CIWP) of present-day GCMs, notably 20th century CMIP5 simulations, and compare these results to CMIP3 and two recent reanalyses. We use three different CloudSat + CALIPSO ice water products and two methods to remove the contribution from the convective core ice mass and/or precipitating cloud hydrometeors with variable sizes and falling speeds so that a robust observational estimate can be obtained for model evaluations. The results show that for annual mean CIWP, there are factors of 2-10 in the differences between observations and models for a majority of the GCMs and for a number of regions. However, there are a number of CMIP5 models, including CNRM-CM5, MRI, CCSM4 and CanESM2, as well as the UCLA CGCM, that perform well compared to our past evaluations. Systematic biases in CIWC vertical structure occur below the mid-troposphere where the models overestimate CIWC, with this bias arising mostly from the extratropics. The tropics are marked by model differences in the level of maximum CIWC (similar to 250-550 hPa). Based on a number of metrics, the ensemble behavior of CMIP5 has improved considerably relative to CMIP3, although neither the CMIP5 ensemble mean nor any individual model performs particularly well, and there are still a number of models that exhibit very large biases despite the availability of relevant observations. The implications of these results on model representations of the Earth radiation balance are discussed, along with caveats and uncertainties associated with the observational estimates, model and observation representations of the precipitating and cloudy ice components, relevant physical processes and parameterizations.
C1 [Li, J-L. F.; Waliser, D. E.; Chen, W-T.; Guan, B.; Kubar, T.; Stephens, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ma, H-Y.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Deng, M.] Univ Wyoming, Laramie, WY 82071 USA.
[Donner, L.; Seman, C.; Horowitz, L.] Princeton Univ, NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08544 USA.
RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, MS 233-306K,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM juilin.f.li@jpl.nasa.gov
RI Guan, Bin/F-6735-2010; Ma, Hsi-Yen/K-1019-2013; Horowitz,
Larry/D-8048-2014; Chen, Wei-Ting/A-4476-2012
OI Horowitz, Larry/0000-0002-5886-3314; Chen, Wei-Ting/0000-0002-9292-0933
FU U.S. Department of Energy by Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]
FX We would like to thank editor and three reviewers for their very
comprehensive review and constructive comments/ suggestion. We thank
Anthony Del Genio/NASA GISS, Ken Lo/NASA GISS, Voldoir Aurore/CNRM,
Masahiro Watanabe and Shingo Watanabe /MIROC, Leon Rotstayn/CSIRO, Knut
von Salzen/CCCma, Gary Strand/NCAR, Alf Kirkevag/NCC, Seiji
Yukimoto/MRI, Jean-Louis Dufresne/IPSL, Tongwen Wu/BCC-CMA and many
other colleagues from climate modeling centers for providing model
information. Thanks also go to Gregory Huey with data and Matthew
Lebsock for reading and providing comments on the manuscript. The
contributions by D.E.W. and J.L.L. to this study were carried out on
behalf of the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. The contribution of Hsi-Yen Ma to this work was
performed under the auspices of the U.S. Department of Energy by
Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344.
NR 77
TC 60
Z9 62
U1 3
U2 42
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 21
PY 2012
VL 117
AR D16105
DI 10.1029/2012JD017640
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 996FY
UT WOS:000308071500002
ER
PT J
AU Allen, CC
Greenhagen, BT
Hanna, KLD
Paige, DA
AF Allen, Carlton C.
Greenhagen, Benjamin T.
Hanna, Kerri L. Donaldson
Paige, David A.
TI Analysis of lunar pyroclastic deposit FeO abundances by LRO Diviner
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID IRON; SURFACE; MOON; SAMPLES; IMAGES; SOILS; MARE
AB Thermal infrared reflectance spectra of rock-forming minerals include a prominent minimum near 8 mu m, known as the "Christiansen feature" (CF). The inflection point wavelength is sensitive to the degree of polymerization of silicates, which is strongly influenced by major cations - notably iron - in the minerals. Laboratory spectra of lunar soils demonstrate that the CF location is closely correlated to the sample's bulk FeO abundance, across the full range of Apollo soil samples, including pyroclastic glass. This correlation is the basis for estimating lunar surface FeO abundances using orbital thermal infrared measurements. The Diviner Lunar Radiometer Experiment on the Lunar Reconnaissance Orbiter includes three thermal infrared channels, selected to determine the CF positions for sites across the lunar surface. Diviner measurements are used to derive FeO abundances in the Aristarchus, Sulpicius Gallus, and Rima Fresnel pyroclastic deposits. The calculated FeO abundances for Aristarchus and Sulpicius Gallus lie within the compositional range of FeO-rich pyroclastic glasses but outside the range of most mare soils, supporting the interpretations of these deposits as glass rich. The calculated FeO abundance for the Rima Fresnel deposit is close to that of mare soils, supporting a contention that this deposit is dominated by basaltic fragments rather than glass. The Diviner measurements hold the potential to determine FeO abundances in many lunar pyroclastic deposits. A better understanding of these compositions will provide insight into the magmatic history and composition of the lunar interior, as well as an enhanced inventory of potential resources for future human exploration.
C1 [Allen, Carlton C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Greenhagen, Benjamin T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Hanna, Kerri L. Donaldson] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
RP Allen, CC (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KT, Houston, TX 77058 USA.
EM carlton.c.allen@nasa.gov
RI Greenhagen, Benjamin/C-3760-2016
FU Lunar Reconnaissance Orbiter Program through Diviner Lunar Radiometer
Experiment
FX We appreciate support from the Lunar Reconnaissance Orbiter Program,
through the Diviner Lunar Radiometer Experiment (David Paige, Principal
Investigator), for each of the authors. We thank Takahiro Hiroi and
Carle Pieters for generously providing the RELAB spectral data and Larry
Taylor for insight into the intricacies of lunar soil. Dorothy Oehler
and Trent Hare improved our understanding of lunar orbital data sets.
Thoughtful reviews by John Delano, Nicolle Zellner, and an anonymous
reviewer considerably improved this manuscript.
NR 43
TC 8
Z9 8
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 AUG 21
PY 2012
VL 117
AR E00H28
DI 10.1029/2011JE003982
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 995LJ
UT WOS:000308009300001
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Baldini, L
Ballet, J
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Bloom, ED
Bonamente, E
Borgland, AW
Bouvier, A
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cecchi, C
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Cillis, AN
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
de Palma, F
Dermer, CD
Digel, SW
Silva, EDE
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Fegan, SJ
Fortin, P
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giordano, F
Glanzman, T
Godfrey, G
Grenier, IA
Guiriec, S
Gustafsson, M
Hadasch, D
Hayashida, M
Hays, E
Hughes, RE
Johannesson, G
Johnson, AS
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Martin, P
Mazziotta, MN
McEnery, JE
Michelson, PF
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nishino, S
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ozaki, M
Parent, D
Persic, M
Pesce-Rollins, M
Petrosian, V
Pierbattista, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Ritz, S
Roth, M
Sbarra, C
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Stawarz, L
Strong, AW
Takahashi, H
Tanaka, T
Thayer, JB
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Vandenbroucke, J
Vianello, G
Vitale, V
Waite, AP
Wood, M
Yang, Z
AF Ackermann, M.
Ajello, M.
Allafort, A.
Baldini, L.
Ballet, J.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cecchi, C.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Cillis, A. N.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
de Palma, F.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Fegan, S. J.
Fortin, P.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giordano, F.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guiriec, S.
Gustafsson, M.
Hadasch, D.
Hayashida, M.
Hays, E.
Hughes, R. E.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Martin, P.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nishino, S.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ozaki, M.
Parent, D.
Persic, M.
Pesce-Rollins, M.
Petrosian, V.
Pierbattista, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Ritz, S.
Roth, M.
Sbarra, C.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Stawarz, Lukasz
Strong, A. W.
Takahashi, H.
Tanaka, T.
Thayer, J. B.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Vandenbroucke, J.
Vianello, G.
Vitale, V.
Waite, A. P.
Wood, M.
Yang, Z.
TI GeV OBSERVATIONS OF STAR-FORMING GALAXIES WITH THE FERMI LARGE AREA
TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; galaxies: starburst; gamma rays: diffuse background; gamma
rays: galaxies
ID GAMMA-RAY EMISSION; ACTIVE GALACTIC NUCLEI; LUMINOUS INFRARED GALAXIES;
DENSE MOLECULAR GAS; SMALL-MAGELLANIC-CLOUD; HIGH-ENERGY EMISSION;
COSMIC-RAY; STARBURST GALAXIES; SPIRAL GALAXIES; RADIO-CONTINUUM
AB Recent detections of the starburst galaxies M82 and NGC 253 by gamma-ray telescopes suggest that galaxies rapidly forming massive stars are more luminous at gamma-ray energies compared to their quiescent relatives. Building upon those results, we examine a sample of 69 dwarf, spiral, and luminous and ultraluminous infrared galaxies at photon energies 0.1-100 GeV using 3 years of data collected by the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (Fermi). Measured fluxes from significantly detected sources and flux upper limits for the remaining galaxies are used to explore the physics of cosmic rays in galaxies. We find further evidence for quasi-linear scaling relations between gamma-ray luminosity and both radio continuum luminosity and total infrared luminosity which apply both to quiescent galaxies of the Local Group and low-redshift starburst galaxies (conservative P-values less than or similar to 0.05 accounting for statistical and systematic uncertainties). The normalizations of these scaling relations correspond to luminosity ratios of log(L0.1-100GeV/L-1.4GHz) = 1.7 +/- 0.1((statistical)) +/- 0.2((dispersion)) and log(L0.1-100GeV/L8-1000 (mu m)) = -4.3 +/- 0.1((statistical)) +/- 0.2((dispersion)) for a galaxy with a star formation rate of 1 M-circle dot yr(-1), assuming a Chabrier initial mass function. Using the relationship between infrared luminosity and gamma-ray luminosity, the collective intensity of unresolved star-forming galaxies at redshifts 0 < z < 2.5 above 0.1 GeV is estimated to be 0.4-2.4 x 10(-6) ph cm(-2) s(-1) sr(-1) (4%-23% of the intensity of the isotropic diffuse component measured with the LAT). We anticipate that similar to 10 galaxies could be detected by their cosmic-ray-induced gamma-ray emission during a 10 year Fermi mission.
C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Pierbattista, M.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Bastieri, D.; Buson, S.; Gustafsson, M.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[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.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.; Razzano, M.; 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.; 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, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.] IN2P3, CNRS, Ecole Polytech, Lab Leprince Ringuet, Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Chekhtman, A.; Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Cillis, A. N.] Parbellon IAFE, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina.
[Cillis, A. N.; Hays, E.; McEnery, J. E.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[Conrad, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Dermer, C. D.; Lovellette, M. N.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Fukazawa, Y.; Nishino, S.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[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.
[Hughes, R. E.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[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, IRAP, UPS OMP, GAHEC, Toulouse, France.
[Longo, F.; Persic, M.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Martin, P.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohno, M.; Ozaki, M.; Stawarz, Lukasz] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Okumura, A.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Persic, M.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM bechtol@stanford.edu; analia.cillis@gmail.com; funk@slac.stanford.edu;
dtorres@ieec.uab.es
RI giglietto, nicola/I-8951-2012; Kuss, Michael/H-8959-2012; Hays,
Elizabeth/D-3257-2012; Funk, Stefan/B-7629-2015; 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; Mazziotta, Mario /O-8867-2015; Reimer,
Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013;
Rando, Riccardo/M-7179-2013; Sgro, Carmelo/K-3395-2016; Torres,
Diego/O-9422-2016; Orlando, E/R-5594-2016;
OI Berenji, Bijan/0000-0002-4551-772X; Gasparrini,
Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; giglietto,
nicola/0000-0002-9021-2888; Funk, Stefan/0000-0002-2012-0080;
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; Mazziotta, Mario /0000-0001-9325-4672; Reimer,
Olaf/0000-0001-6953-1385; Torres, Diego/0000-0002-1522-9065; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Rando,
Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862;
Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Cutini, Sara/0000-0002-1271-2924
FU K. A. Wallenberg Foundation; Stanford Graduate Fellowship
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; K.B. thanks Eric Feigelson of the
Penn State Center for Astrostatistics for suggestions regarding the
analysis of partially censored data sets. K. B. is supported by a
Stanford Graduate Fellowship.
NR 150
TC 114
Z9 115
U1 1
U2 16
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 20
PY 2012
VL 755
IS 2
AR 164
DI 10.1088/0004-637X/755/2/164
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400081
ER
PT J
AU Aliu, E
Archambault, S
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bottcher, M
Bouvier, A
Bugaev, V
Cannon, A
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Dumm, J
Errando, M
Falcone, A
Federici, S
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
Hui, CM
Imran, A
Jameil, O
Kaaret, P
Karlsson, N
Kertzman, M
Kerr, J
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
Lee, K
Madhavan, AS
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Nelson, T
de Bhroithe, AO
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pichel, A
Pohl, M
Quinn, J
Ragan, K
Reynolds, PT
Roache, E
Ruppel, J
Saxon, DB
Schroedter, M
Sembroski, GH
Senturk, GD
Smith, AW
Staszak, D
Stroh, M
Telezhinsky, I
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Varlotta, A
Vassiliev, VV
Vivier, M
Wakely, SP
Ward, JE
Weinstein, A
Welsing, R
Williams, DA
Zitzer, B
AF Aliu, E.
Archambault, S.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Boettcher, M.
Bouvier, A.
Bugaev, V.
Cannon, A.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickherber, R.
Dumm, J.
Errando, M.
Falcone, A.
Federici, S.
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.
Hui, C. M.
Imran, A.
Jameil, O.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kerr, J.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
Lee, K.
Madhavan, A. S.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Nelson, T.
de Bhroithe, A. O'Faolain
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pichel, A.
Pohl, M.
Quinn, J.
Ragan, K.
Reynolds, P. T.
Roache, E.
Ruppel, J.
Saxon, D. B.
Schroedter, M.
Sembroski, G. H.
Sentuerk, G. D.
Smith, A. W.
Staszak, D.
Stroh, M.
Telezhinsky, I.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Varlotta, A.
Vassiliev, V. V.
Vivier, M.
Wakely, S. P.
Ward, J. E.
Weinstein, A.
Welsing, R.
Williams, D. A.
Zitzer, B.
TI MULTIWAVELENGTH OBSERVATIONS OF THE AGN 1ES 0414+009 WITH VERITAS,
FERMI-LAT, SWIFT-XRT, AND MDM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (1ES 0414+009, ERJ0416+011); gamma rays:
galaxies
ID BL LACERTAE OBJECT; GAMMA-RAY ASTRONOMY; TELESCOPE; EMISSION; SEARCH;
DISCOVERY; BLAZARS; SAMPLE; STARS
AB We present observations of the BL Lac object 1ES 0414+009 in the >200 GeV gamma-ray band by the VERITAS array of Cherenkov telescopes. 1ES 0414+009 was observed by VERITAS between 2008 January and 2011 February, resulting in 56.2 hr of good quality pointed observations. These observations resulted in a detection of 822 events from the source corresponding to a statistical significance of 6.4 standard deviations (6.4 sigma) above the background. The source flux, showing no evidence for variability, is measured as (5.2 +/- 1.1(stat) +/- 2.6(sys)) x 10(-12) photons cm(-2) s(-1) above 200 GeV, equivalent to approximately 2% of the Crab Nebula flux above this energy. The differential photon spectrum from 230 GeV to 850 GeV is well fit by a power law with a photon index of Gamma = 3.4 +/- 0.5(stat) +/- 0.3(sys) and a flux normalization of (1.6 +/- 0.3(stat) +/- 0.8(sys)) x 10(-11) photons cm(-2) s(-1) at 300 GeV. We also present multiwavelength results taken in the optical (MDM), x-ray (Swift-XRT), and GeV (Fermi-LAT) bands and use these results to construct a broadband spectral energy distribution (SED). Modeling of this SED indicates that homogenous one-zone leptonic scenarios are not adequate to describe emission from the system, with a lepto-hadronic model providing a better fit to the data.
C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Archambault, S.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] 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.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.; Ward, J. E.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Boettcher, M.; Jameil, O.; Kerr, J.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA.
[Cannon, A.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] 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.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Federici, S.; Hughes, G.; Pohl, M.; Ruppel, J.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany.
[Federici, S.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Gall, D.; Kaaret, P.; Stroh, M.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Huan, H.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Imran, A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin, 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.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[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.
[Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
EM aw.smith@utah.edu
RI Khassen, Yerbol/I-3806-2015;
OI Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794;
Lang, Mark/0000-0003-4641-4201; Khassen, Yerbol/0000-0002-7296-3100;
Cui, Wei/0000-0002-6324-5772
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 U.K.
FX 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 U.K. 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. This work also made use of
data supplied by the UK Swift Science Data Centre at the University of
Leicester.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2012
VL 755
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AR 118
DI 10.1088/0004-637X/755/2/118
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400035
ER
PT J
AU Becker, W
Prinz, T
Winkler, PF
Petre, R
AF Becker, Werner
Prinz, Tobias
Winkler, P. Frank
Petre, Robert
TI THE PROPER MOTION OF THE CENTRAL COMPACT OBJECT RX J0822-4300 IN THE
SUPERNOVA REMNANT PUPPIS A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (RX J0822-4300); stars: neutron; X-rays: stars
ID NEUTRON-STAR KICKS; PULSAR; EXPLOSIONS; G292.0+1.8; DISCOVERY; BIRTH
AB Using the High Resolution Camera on board the Chandra X-ray Observatory, we have re-examined the proper motion of the central compact object RX J0822-4300 in the supernova remnant Puppis A. New data from 2010 August, combined with three archival data sets from as early as 1999 December, provide a baseline of 3886 days (more than 10.5 yr) to perform the measurement. Correlating the four positions of RX J0822-4300 measured in each data set implies a projected proper motion of mu = 71 +/- 12 mas yr(-1). For a distance of 2 kpc, this proper motion is equivalent to a recoil velocity of 672 +/- 115 km s(-1). The position angle is found to be 244 degrees +/- 11 degrees. Both the magnitude and direction of the proper motion are in agreement with RX J0822-4300 originating near the optical expansion center of the supernova remnant. For a displacement of 371 +/- 31 arcsec between its birthplace and today's position, we deduce an age of (5.2 +/- 1.0) x 10(3) yr for RX J0822-4300. The age inferred from the neutron star proper motion and filament motions can be considered as two independent measurements of the same quantity. They average to 4450 +/- 750 yr for the age of the supernova remnant Puppis A.
C1 [Becker, Werner; Prinz, Tobias] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Becker, Werner] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Becker, W (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85741 Garching, Germany.
FU International Max-Planck Research School on Astrophysics at the
Ludwig-Maximilians University, IMPRS; NSF [AST-0908566]
FX T.P. acknowledges support by the International Max-Planck Research
School on Astrophysics at the Ludwig-Maximilians University, IMPRS; P.
F. W. acknowledges support from the NSF through grant AST-0908566. We
are grateful to Daniel Patnaude for his contributions in scheduling and
setting up the observations and to several members of the HelpDesk staff
at the Chandra X-ray Center for assistance at various stages of this
project, and especially for helping to sort out the troublesome software
bug described in Section 2.1. We also acknowledge the use of the Chandra
data archive.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2012
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DI 10.1088/0004-637X/755/2/141
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SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400058
ER
PT J
AU Chandra, P
Chevalier, RA
Chugai, N
Fransson, C
Irwin, CM
Soderberg, AM
Chakraborti, S
Immler, S
AF Chandra, Poonam
Chevalier, Roger A.
Chugai, Nikolai
Fransson, Claes
Irwin, Christopher M.
Soderberg, Alicia M.
Chakraborti, Sayan
Immler, Stefan
TI RADIO AND X-RAY OBSERVATIONS OF SN 2006jd: ANOTHER STRONGLY INTERACTING
TYPE IIn SUPERNOVA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; hydrodynamics; radio continuum: general; stars:
mass-loss; supernovae: general; supernovae: individual (SN 2006jd)
ID PARTICLE-ACCELERATION; GALAXY NGC-891; EMISSION; SN-1988Z; STAR;
INSTABILITIES; ABSORPTION; EVOLUTION; REMNANTS; SPECTRA
AB We report four years of radio and X-ray monitoring of the Type IIn supernova SN 2006jd at radio wavelengths with the Very Large Array, Giant Metrewave Radio Telescope, and Expanded Very Large Array; at X-ray wavelengths with Chandra, XMM-Newton, and Swift-XRT. We assume that the radio and X-ray emitting particles are produced by shock interaction with a dense circumstellar medium. The radio emission shows an initial rise that can be attributed to free-free absorption by cool gas mixed into the nonthermal emitting region; external free-free absorption is disfavored because of the shape of the rising light curves and the low gas column density inferred along the line of sight to the emission region. The X-ray luminosity implies a preshock circumstellar density similar to 10(6) cm(-3) at a radius r similar to 2 x 10(16) cm, but the column density inferred from the photoabsorption of X-rays along the line of sight suggests a significantly lower density. The implication may be an asymmetry in the interaction. The X-ray spectrum shows Fe line emission at 6.9 keV that is stronger than is expected for the conditions in the X-ray emitting gas. We suggest that cool gas mixed into the hot gas plays a role in the line emission. Our radio and X-ray data both suggest the density profile is flatter than r(-2) because of the slow evolution of the unabsorbed emission.
C1 [Chandra, Poonam] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada.
[Chevalier, Roger A.; Irwin, Christopher M.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Chugai, Nikolai] Russian Acad Sci, Inst Astron, Moscow 109017, Russia.
[Fransson, Claes] Stockholm Univ, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden.
[Soderberg, Alicia M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Chakraborti, Sayan] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India.
[Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Immler, Stefan] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Immler, Stefan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Chandra, P (reprint author), Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada.
EM Poonam.Chandra@rmc.ca
FU NSERC; NASA [NNX09AH58G, GO9-0079X]; NSF [AST-0807727]
FX P.C. and R. C. are grateful to Craig Sarazin for discussions on X-ray
emission and analysis. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. P. C. is supported by her
NSERC Discovery grants. R. C. and C. I. acknowledge support from NASA
grants NNX09AH58G (XMM) and GO9-0079X (Chandra), and NSF grant
AST-0807727.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2012
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DI 10.1088/0004-637X/755/2/110
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400027
ER
PT J
AU Eisenhardt, PRM
Wu, JW
Tsai, CW
Assef, R
Benford, D
Blain, A
Bridge, C
Condon, JJ
Cushing, MC
Cutri, R
Evans, NJ
Gelino, C
Griffith, RL
Grillmair, CJ
Jarrett, T
Lonsdale, CJ
Masci, FJ
Mason, BS
Petty, S
Sayers, J
Stanford, SA
Stern, D
Wright, EL
Yan, L
AF Eisenhardt, Peter R. M.
Wu, Jingwen
Tsai, Chao-Wei
Assef, Roberto
Benford, Dominic
Blain, Andrew
Bridge, Carrie
Condon, J. J.
Cushing, Michael C.
Cutri, Roc
Evans, Neal J., II
Gelino, Chris
Griffith, Roger L.
Grillmair, Carl J.
Jarrett, Tom
Lonsdale, Carol J.
Masci, Frank J.
Mason, Brian S.
Petty, Sara
Sayers, Jack
Stanford, S. A.
Stern, Daniel
Wright, Edward L.
Yan, Lin
TI THE FIRST HYPER-LUMINOUS INFRARED GALAXY DISCOVERED BY WISE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (WISE J181417.29+341224.9); infrared: galaxies
ID SPECTRAL ENERGY-DISTRIBUTIONS; DIGITAL-SKY-SURVEY; BLACK-HOLE MASS;
ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; SURVEY-EXPLORER WISE;
SPACE-TELESCOPE; FSC 10214+4724; MU-M; QUASAR
AB We report the discovery by the Wide-field Infrared Survey Explorer (WISE) of the z = 2.452 source WISE J181417.29+341224.9, the first hyperluminous source found in the WISE survey. WISE 1814+3412 is also the prototype for an all-sky sample of similar to 1000 extremely luminous "W1W2-dropouts" (sources faint or undetected by WISE at 3.4 and 4.6 mu m and well detected at 12 or 22 mu m). The WISE data and a 350 mu m detection give a minimum bolometric luminosity of 3.7 x 10(13) L-circle dot, with similar to 10(14) L-circle dot plausible. Follow-up images reveal four nearby sources: a QSO and two Lyman break galaxies (LBGs) at z = 2.45, and an M dwarf star. The brighter LBG dominates the bolometric emission. Gravitational lensing is unlikely given the source locations and their different spectra and colors. The dominant LBG spectrum indicates a star formation rate similar to 300 M-circle dot yr(-1), accounting for less than or similar to 10% of the bolometric luminosity. Strong 22 mu m emission relative to 350 mu m implies that warm dust contributes significantly to the luminosity, while cooler dust normally associated with starbursts is constrained by an upper limit at 1.1 mm. Radio emission is similar to 10 times above the far-infrared/radio correlation, indicating an active galactic nucleus (AGN) is present. An obscured AGN combined with starburst and evolved stellar components can account for the observations. If the black hole mass follows the local M-BH-bulge mass relation, the implied Eddington ratio is greater than or similar to 4. WISE 1814+3412 may be a heavily obscured object where the peak AGN activity occurred prior to the peak era of star formation.
C1 [Eisenhardt, Peter R. M.; Wu, Jingwen; Assef, Roberto; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tsai, Chao-Wei; Cutri, Roc; Gelino, Chris; Griffith, Roger L.; Grillmair, Carl J.; Jarrett, Tom; Masci, Frank J.; Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Benford, Dominic] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blain, Andrew] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Bridge, Carrie; Sayers, Jack] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Condon, J. J.; Lonsdale, Carol J.; Mason, Brian S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Evans, Neal J., II] Univ Texas Austin, Dept Astron, Dept Phys & Astron, Austin, TX 78712 USA.
[Petty, Sara; Wright, Edward L.] Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA.
[Stanford, S. A.] Univ Calif Davis, Davis, CA 95616 USA.
RP Eisenhardt, PRM (reprint author), CALTECH, Jet Prop Lab, MS 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Peter.R.Eisenhardt@jpl.nasa.gov
RI Benford, Dominic/D-4760-2012
OI Benford, Dominic/0000-0002-9884-4206
FU NSF [AST-1109116]; National Aeronautics and Space Administration; W. M.
Keck Foundation; NASA Postdoctoral Program at the Jet Propulsion
Laboratory
FX R.J.A. and J.W. were 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. N.J.E.
acknowledges support from NSF Grant AST-1109116. This publication makes
use of data products from the Wide-field Infrared Survey Explorer, which
is a joint project of the University of California, Los Angeles, and the
Jet Propulsion Laboratory/California Institute of Technology, funded by
the National Aeronautics and Space Administration. This work is based in
part on observations made with the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology under contract with NASA. Some of the data presented here
were obtained at the W. M. Keck Observatory, which is operated as a
scientific partnership among Caltech, the University of California and
NASA. The Keck Observatory was made possible by the generous financial
support of the W. M. Keck Foundation. Some of the data are based on
observations obtained at the Hale Telescope, Palomar Observatory as part
of a continuing collaboration between the California Institute of
Technology, NASA/JPL, and Cornell University. Some of the data presented
here were obtained at 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. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2012
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DI 10.1088/0004-637X/755/2/173
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400090
ER
PT J
AU Godfrey, LEH
Bicknell, GV
Lovell, JEJ
Jauncey, DL
Gelbord, J
Schwartz, DA
Perlman, ES
Marshall, HL
Birkinshaw, M
Worrall, DM
Georganopoulos, M
Murphy, DW
AF Godfrey, L. E. H.
Bicknell, G. V.
Lovell, J. E. J.
Jauncey, D. L.
Gelbord, J.
Schwartz, D. A.
Perlman, E. S.
Marshall, H. L.
Birkinshaw, M.
Worrall, D. M.
Georganopoulos, M.
Murphy, D. W.
TI A MULTI-WAVELENGTH STUDY OF THE JET, LOBES, AND CORE OF THE QUASAR PKS
2101-490
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: jets; quasars: individual (PKS 2101-490)
ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE;
LARGE-SCALE JETS; II RADIO-SOURCES; MAGNETIC-FIELD STRENGTHS;
INVERSE-COMPTON MODEL; HOT-SPOTS; CHANDRA OBSERVATIONS; IMAGING SURVEY
AB We present a detailed study of the x-ray, optical, and radio emission from the jet, lobes, and core of the quasar PKS 2101-490 as revealed by new Chandra, Hubble Space Telescope (HST), and ATCA images. We extract the radio to x-ray spectral energy distributions from seven regions of the 13 '' jet, and model the jet x-ray emission in terms of Doppler beamed inverse Compton scattering of the cosmic microwave background (IC/CMB) for a jet in a state of equipartition between particle and magnetic field energy densities. This model implies that the jet remains highly relativistic hundreds of kiloparsecs from the nucleus, with a bulk Lorentz factor Gamma similar to 6 and magnetic field of the order of 30 mu G. We detect an apparent radiative cooling break in the synchrotron spectrum of one of the jet knots, and are able to interpret this in terms of a standard one-zone continuous injection model, based on jet parameters derived from the IC/CMB model. However, we note apparent substructure in the bright optical knot in one of the HST bands. We confront the IC/CMB model with independent estimates of the jet power, and find that the IC/CMB model jet power is consistent with the independent estimates, provided that the minimum electron Lorentz factor gamma(min) greater than or similar to 50, and the knots are significantly longer than the jet width, as implied by de-projection of the observed knot lengths.
C1 [Godfrey, L. E. H.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6102, Australia.
[Godfrey, L. E. H.; Bicknell, G. V.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Lovell, J. E. J.; Jauncey, D. L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia.
[Lovell, J. E. J.] CSIRO, Ind Phys, Lindfield, NSW 2070, Australia.
[Lovell, J. E. J.] Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia.
[Gelbord, J.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Schwartz, D. A.; Birkinshaw, M.; Worrall, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Marshall, H. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Birkinshaw, M.; Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Georganopoulos, M.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA.
[Murphy, D. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Godfrey, LEH (reprint author), Curtin Univ Technol, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6102, Australia.
EM L.Godfrey@curtin.edu.au
RI Godfrey, Leith/B-5283-2013
FU Grote Reber Foundation; HST [GO-10352]; NASA [NAS8-03060]; CXC
[GO9-0121B]; Commonwealth of Australia
FX L.E.H.G thanks the Grote Reber Foundation for financial support during
part of this work. H. L. M., E. S. P., and J.G. acknowledge the support
of HST grant GO-10352. D. A. S. is supported by NASA contract NAS8-03060
and CXC grant GO9-0121B. The Australia Telescope Compact Array is part
of the Australia Telescope which is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO. We
gratefully acknowledge the anonymous referee for their comments which
helped to improve and clarify the manuscript.
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U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2012
VL 755
IS 2
AR 174
DI 10.1088/0004-637X/755/2/174
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400091
ER
PT J
AU Rujopakarn, W
Rieke, GH
Papovich, CJ
Weiner, BJ
Rigby, JR
Rex, M
Bian, F
Kuhn, OP
Thompson, D
AF Rujopakarn, W.
Rieke, G. H.
Papovich, C. J.
Weiner, B. J.
Rigby, J. R.
Rex, M.
Bian, F.
Kuhn, O. P.
Thompson, D.
TI LARGE BINOCULAR TELESCOPE AND SPITZER SPECTROSCOPY OF STAR-FORMING
GALAXIES AT 1 < z < 3: EXTINCTION AND STAR FORMATION RATE INDICATORS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst;
infrared: galaxies
ID INFRARED LUMINOSITY FUNCTIONS; SIMILAR-TO 2.5; GRAVITATIONALLY LENSED
GALAXY; MULTIBAND IMAGING PHOTOMETER; INITIAL MASS FUNCTION; LYMAN BREAK
GALAXY; 8 OCLOCK ARC; HIGH-REDSHIFT; MIDINFRARED SPECTROSCOPY; SMM
J163554.2+661225
AB We present spectroscopic observations in the rest-frame optical and near- to mid-infrared wavelengths of four gravitationally lensed infrared (IR) luminous star-forming galaxies at redshift 1 < z < 3 from the LUCIFER instrument on the Large Binocular Telescope and the Infrared Spectrograph on Spitzer. The sample was selected to represent pure, actively star-forming systems, absent of active galactic nuclei. The large lensing magnifications result in high signal-to-noise spectra that can probe faint IR recombination lines, including Pa alpha and Br alpha at high redshifts. The sample was augmented by three lensed galaxies with similar suites of unpublished data and observations from the literature, resulting in the final sample of seven galaxies. We use the IR recombination lines in conjunction with H alpha observations to probe the extinction, A(v), of these systems, as well as testing star formation rate (SFR) indicators against the SFR measured by fitting spectral energy distributions to far-IR photometry. Our galaxies occupy a range of A(v) from similar to 0 to 5.9 mag, larger than previously known for a similar range of IR luminosities at these redshifts. Thus, estimates of SFR even at z similar to 2 must take careful count of extinction in the most IR luminous galaxies. We also measure extinction by comparing SFR estimates from optical emission lines with those from far-IR measurements. The comparison of results from these two independent methods indicates a large variety of dust distribution scenarios at 1 < z < 3. Without correcting for dust extinction, the H alpha SFR indicator underestimates the SFR; the size of the necessary correction depends on the IR luminosity and dust distribution scenario. Individual SFR estimates based on the 6.2 mu m polycyclic aromatic hydrocarbon emission line luminosity do not show a systematic discrepancy with extinction, although a considerable, similar to 0.2 dex, scatter is observed.
C1 [Rujopakarn, W.; Rieke, G. H.; Weiner, B. J.; Rex, M.; Bian, F.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Papovich, C. J.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Rigby, J. R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Kuhn, O. P.; Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA.
RP Rujopakarn, W (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
EM wiphu@as.arizona.edu
RI Rigby, Jane/D-4588-2012;
OI Rigby, Jane/0000-0002-7627-6551; Rujopakarn, Wiphu/0000-0002-0303-499X
FU Thai Government; Caltech/JPL [1255094]
FX We thank Brian Siana and Eiichi Egami for helpful discussions. W. R.
thanks Alexandra Pope and Philip Choi for data points in Figures 6 and
7, respectively, and acknowledges the support from the Thai Government
Scholarship. This work is supported by contract 1255094 from Caltech/JPL
to the University of Arizona.
NR 59
TC 11
Z9 11
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 AUG 20
PY 2012
VL 755
IS 2
AR 168
DI 10.1088/0004-637X/755/2/168
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400085
ER
PT J
AU Sargsyan, L
Lebouteiller, V
Weedman, D
Spoon, H
Bernard-Salas, J
Engels, D
Stacey, G
Houck, J
Barry, D
Miles, J
Samsonyan, A
AF Sargsyan, L.
Lebouteiller, V.
Weedman, D.
Spoon, H.
Bernard-Salas, J.
Engels, D.
Stacey, G.
Houck, J.
Barry, D.
Miles, J.
Samsonyan, A.
TI [C II] 158 mu m LUMINOSITIES AND STAR FORMATION RATE IN DUSTY STARBURSTS
AND ACTIVE GALACTIC NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: distances and redshifts; galaxies:
starburst; infrared: galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; POLYCYCLIC
AROMATIC-HYDROCARBONS; MIDINFRARED SPECTROSCOPY; SUBMILLIMETER GALAXIES;
PHOTODISSOCIATION REGIONS; LUMINOUS STARBURSTS; INTERSTELLAR-MEDIUM;
EARLY UNIVERSE; HIGH-REDSHIFT
AB Results are presented for [C II] 158 mu m line fluxes observed with the Herschel PACS instrument in 112 sources with both starburst and active galactic nucleus (AGN) classifications, of which 102 sources have confident detections. Results are compared with mid-infrared spectra from the Spitzer Infrared Spectrometer and with L-ir from IRAS fluxes; AGN/starburst classifications are determined from equivalent width of the 6.2 mu m polycyclic aromatic hydrocarbon (PAH) feature. It is found that the [CII] line flux correlates closely with the flux of the 11.3 mu m PAH feature independent of AGN/starburst classification, log [f([C II] 158 mu m)/f(11.3 mu m PAH)] = -0.22 +/- 0.25. It is concluded that the [CII] line flux measures the photodissociation region associated with starbursts in the same fashion as the PAH feature. A calibration of star formation rate (SFR) for the starburst component in any source having [C II] is derived comparing [C II] luminosity L([C II]) to L-ir with the result that log SFR = log L([C II)]) -7.08 +/- 0.3, for SFR in M-circle dot yr(-1) and L([C II]) in L-circle dot. The decreasing ratio of L([C II]) to L-ir in more luminous sources (the "[C II] deficit") is shown to be a consequence of the dominant contribution to L-ir arising from a luminous AGN component because the sources with the largest L-ir and smallest L([C II])/L-ir are AGNs.
C1 [Sargsyan, L.; Weedman, D.; Spoon, H.; Stacey, G.; Houck, J.; Barry, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Lebouteiller, V.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,DAPINA,Serv Astrophys, Saclay, France.
[Bernard-Salas, J.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Engels, D.] Hamburger Sternwarte, Hamburg, Germany.
[Miles, J.] NASA, Ames Res Ctr, SOFIA, USRA, Moffett Field, CA 94035 USA.
[Samsonyan, A.] Byurakan Astrophys Observ, Byurakan, Armenia.
RP Sargsyan, L (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM sargsyan@isc.astro.cornell.edu; vianney.lebouteiller@cea.fr;
dweedman@isc.astro.cornell.edu
FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain); NASA; Deutsche
Forschungsgemeinschaft [En 176/36-1]; Marie Curie Intra-European
Fellowship within the 7th European Community Framework Program [272820]
FX We thank those who developed the Herschel Observatory for the
opportunity to observe with open time. 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); and IAC (Spain).
This development was supported by the funding agencies BMVIT (Austria),
ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF
(Italy), and CICYT/MCYT (Spain). Support for this work by the IRS GTO
team and Herschel observing team at Cornell University was provided by
NASA through Contracts issued by JPL/Caltech and by the NASA Herschel
Science Center. L. S. also acknowledges support from the Deutsche
Forschungsgemeinschaft grant En 176/36-1. J.B.S. acknowledges support
from a Marie Curie Intra-European Fellowship within the 7th European
Community Framework Program under project number 272820.
NR 68
TC 42
Z9 42
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 AUG 20
PY 2012
VL 755
IS 2
AR 171
DI 10.1088/0004-637X/755/2/171
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400088
ER
PT J
AU Seymour, N
Altieri, B
De Breuck, C
Barthel, P
Coia, D
Conversi, L
Dannerbauer, H
Dey, A
Dickinson, M
Drouart, G
Galametz, A
Greve, TR
Haas, M
Hatch, N
Ibar, E
Ivison, R
Jarvis, M
Kovacs, A
Kurk, J
Lehnert, M
Miley, G
Nesvadba, N
Rawlings, JI
Rettura, A
Rottgering, H
Rocca-Volmerange, B
Sanchez-Portal, M
Santos, JS
Stern, D
Stevens, J
Valtchanov, I
Vernet, J
Wylezalek, D
AF Seymour, N.
Altieri, B.
De Breuck, C.
Barthel, P.
Coia, D.
Conversi, L.
Dannerbauer, H.
Dey, A.
Dickinson, M.
Drouart, G.
Galametz, A.
Greve, T. R.
Haas, M.
Hatch, N.
Ibar, E.
Ivison, R.
Jarvis, M.
Kovacs, A.
Kurk, J.
Lehnert, M.
Miley, G.
Nesvadba, N.
Rawlings, J. I.
Rettura, A.
Rottgering, H.
Rocca-Volmerange, B.
Sanchez-Portal, M.
Santos, J. S.
Stern, D.
Stevens, J.
Valtchanov, I.
Vernet, J.
Wylezalek, D.
TI RAPID COEVAL BLACK HOLE AND HOST GALAXY GROWTH IN MRC 1138-262: THE
HUNGRY SPIDER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: formation; galaxies: high-redshift;
galaxies: individual (MRC 1138-262)
ID REDSHIFT RADIO GALAXIES; ACTIVE GALACTIC NUCLEI; SIMILAR-TO 2; SPECTRAL
ENERGY-DISTRIBUTIONS; FAR-INFRARED PROPERTIES; STAR-FORMING GALAXIES;
BULGE MASS RELATION; H-ALPHA EMITTERS; K-Z RELATION; ELLIPTIC GALAXIES
AB We present a detailed study of the infrared spectral energy distribution of the high-redshift radio galaxy MRC 1138-26 at z = 2.156, also known as the Spiderweb Galaxy. By combining photometry from Spitzer, Herschel, and LABOCA we fit the rest-frame 5-300 mu m emission using a two-component, starburst, and active galactic nucleus (AGN) model. The total infrared (8-1000 mu m) luminosity of this galaxy is (1.97 +/- 0.28) x 10(13) L-circle dot with (1.17 +/- 0.27) and (0.79 +/- 0.09) x 10(13) L-circle dot due to the AGN and starburst components, respectively. The high derived AGN accretion rate of similar to 20% Eddington and the measured star formation rate (SFR) of 1390 +/- 150 M-circle dot yr(-1) suggest that this massive system is in a special phase of rapid central black hole and host galaxy growth, likely caused by a gas-rich merger in a dense environment. The accretion rate is sufficient to power both the jets and the previously observed large outflow. The high SFR and strong outflow suggest that this galaxy could potentially exhaust its fuel for stellar growth in a few tens of Myr, although the likely merger of the radio galaxy with nearby satellites suggests that bursts of star formation may recur again on timescales of several hundreds of Myr. The age of the radio lobes implies the jet started after the current burst of star formation, and therefore we are possibly witnessing the transition from a merger-induced starburst phase to a radio-loud AGN phase. We also note tentative evidence for [CII] 158 mu m emission. This paper marks the first results from the Herschel Galaxy Evolution Project (Project HeRGE), a systematic study of the evolutionary state of 71 high-redshift, 1 < z < 5.2, radio galaxies.
C1 [Seymour, N.; Drouart, G.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Seymour, N.; Rawlings, J. I.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Altieri, B.; Coia, D.; Conversi, L.; Sanchez-Portal, M.; Santos, J. S.; Valtchanov, I.] ESA, European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain.
[De Breuck, C.; Drouart, G.; Vernet, J.; Wylezalek, D.] European So Observ, D-85748 Garching, Germany.
[Barthel, P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Dannerbauer, H.] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria.
[Dey, A.; Dickinson, M.] NOAO Tucson, Tucson, AZ 85719 USA.
[Drouart, G.; Rocca-Volmerange, B.] Inst Astrophys, F-75014 Paris, France.
[Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Haas, M.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany.
[Hatch, N.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Ibar, E.; Ivison, R.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R.; Stevens, J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Jarvis, M.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[Kovacs, A.] Univ Minnesota, Dept Astron, Minneapolis, MN 55414 USA.
[Kurk, J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Lehnert, M.; Nesvadba, N.] Univ Paris Diderot, Observ Paris, CNRS, GEPI,UMR 8111, F-92190 Meudon, France.
[Miley, G.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Rettura, A.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Seymour, N (reprint author), CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia.
RI Drouart, Guillaume/C-6049-2016; Kovacs, Attila/C-1171-2010; Ivison,
R./G-4450-2011;
OI Drouart, Guillaume/0000-0003-2275-5466; Kovacs,
Attila/0000-0001-8991-9088; Ivison, R./0000-0001-5118-1313; Hatch,
Nina/0000-0001-5600-0534; Vernet, Joel/0000-0002-8639-8560; Seymour,
Nicholas/0000-0003-3506-5536; De Breuck, Carlos/0000-0002-6637-3315;
Altieri, Bruno/0000-0003-3936-0284
FU Australian Research Council; Science and Technologies Facilities
Council; IDA; DARK; NASA through JPL/Caltech
FX N.S. is the recipient of an Australian Research Council Future
Fellowship. T. R. G. acknowledges support from the Science and
Technologies Facilities Council, as well as IDA and DARK. We thank J.
Mullaney for help using the DecompIR code. 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. HIPE is a joint development by the
Herschel Science Ground Segment Consortium, consisting of ESA, the NASA
Herschel Science Center, and the HIFI, PACS, and SPIRE consortia
NR 80
TC 31
Z9 31
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 AUG 20
PY 2012
VL 755
IS 2
AR 146
DI 10.1088/0004-637X/755/2/146
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400063
ER
PT J
AU Shin, IG
Han, C
Choi, JY
Udalski, A
Sumi, T
Gould, A
Bozza, V
Dominik, M
Fouque, P
Horne, K
Szymanski, MK
Kubiak, M
Soszynski, I
Pietrzynski, G
Poleski, R
Ulaczyk, K
Pietrukowicz, P
Kozllowski, S
Skowron, J
Wyrzykowski, L
Collaboration, O
Abe, F
Bennett, DP
Bond, IA
Botzler, CS
Chote, P
Freeman, M
Fukui, A
Furusawa, K
Itow, Y
Kobara, S
Ling, CH
Masuda, K
Matsubara, Y
Miyake, N
Muraki, Y
Ohmori, K
Ohnishi, K
Rattenbury, NJ
Saito, T
Sullivan, DJ
Suzuki, D
Suzuki, K
Sweatman, WL
Takino, S
Tristram, PJ
Wada, K
Yock, PCM
Bramich, DM
Snodgrass, C
Steele, IA
Street, RA
Tsapras, Y
Alsubai, KA
Browne, P
Burgdorf, MJ
Novati, SC
Dodds, P
Dreizler, S
Fang, XS
Grundahl, F
Gu, CH
Hardis, S
Harpsoe, K
Hinse, TC
Hornstrup, A
Hundertmark, M
Jessen-Hansen, J
Jorgensen, UG
Kains, N
Kerins, E
Liebig, C
Lund, M
Lunkkvist, M
Mancini, L
Mathiasen, M
Penny, MT
Rahvar, S
Ricci, D
Scarpetta, G
Skottfelt, J
Southworth, J
Surdej, J
Tregloan-Reed, J
Wambsganss, J
Wertz, O
Almeida, LA
Batista, V
Christie, G
Depoy, DL
Dong, S
Gaudi, BS
Henderson, C
Jablonski, F
Lee, CU
McCormick, J
McGregor, D
Moorhouse, D
Natusch, T
Ngan, H
Park, SY
Pogge, RW
Tan, TG
Thornley, G
Yee, JC
Albrow, MD
Bachelet, E
Beaulieu, JP
Brillant, S
Cassan, A
Cole, AA
Corrales, E
Coutures, C
Dieters, S
Prester, DD
Donatowicz, J
Greenhill, J
Kubas, D
Marquette, JB
Menzies, JW
Sahu, KC
Zub, M
AF Shin, I. -G.
Han, C.
Choi, J. -Y.
Udalski, A.
Sumi, T.
Gould, A.
Bozza, V.
Dominik, M.
Fouque, P.
Horne, K.
Szymanski, M. K.
Kubiak, M.
Soszynski, I.
Pietrzynski, G.
Poleski, R.
Ulaczyk, K.
Pietrukowicz, P.
Kozllowski, S.
Skowron, J.
Wyrzykowski, L.
Collaboration, Ogle
Abe, F.
Bennett, D. P.
Bond, I. A.
Botzler, C. S.
Chote, P.
Freeman, M.
Fukui, A.
Furusawa, K.
Itow, Y.
Kobara, S.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Miyake, N.
Muraki, Y.
Ohmori, K.
Ohnishi, K.
Rattenbury, N. J.
Saito, To.
Sullivan, D. J.
Suzuki, D.
Suzuki, K.
Sweatman, W. L.
Takino, S.
Tristram, P. J.
Wada, K.
Yock, P. C. M.
Bramich, D. M.
Snodgrass, C.
Steele, I. A.
Street, R. A.
Tsapras, Y.
Alsubai, K. A.
Browne, P.
Burgdorf, M. J.
Novati, S. Calchi
Dodds, P.
Dreizler, S.
Fang, X. -S.
Grundahl, F.
Gu, C. -H.
Hardis, S.
Harpsoe, K.
Hinse, T. C.
Hornstrup, A.
Hundertmark, M.
Jessen-Hansen, J.
Jorgensen, U. G.
Kains, N.
Kerins, E.
Liebig, C.
Lund, M.
Lunkkvist, M.
Mancini, L.
Mathiasen, M.
Penny, M. T.
Rahvar, S.
Ricci, D.
Scarpetta, G.
Skottfelt, J.
Southworth, J.
Surdej, J.
Tregloan-Reed, J.
Wambsganss, J.
Wertz, O.
Almeida, L. A.
Batista, V.
Christie, G.
DePoy, D. L.
Dong, Subo
Gaudi, B. S.
Henderson, C.
Jablonski, F.
Lee, C. -U.
McCormick, J.
McGregor, D.
Moorhouse, D.
Natusch, T.
Ngan, H.
Park, S. -Y.
Pogge, R. W.
Tan, T. -G.
Thornley, G.
Yee, J. C.
Albrow, M. D.
Bachelet, E.
Beaulieu, J. -P.
Brillant, S.
Cassan, A.
Cole, A. A.
Corrales, E.
Coutures, C.
Dieters, S.
Prester, D. Dominis
Donatowicz, J.
Greenhill, J.
Kubas, D.
Marquette, J. -B.
Menzies, J. W.
Sahu, K. C.
Zub, M.
CA MOA Collaboration
RoboNet Collaboration
MiNDSTEp Consortium
FUN Collaboration
PLANET Collaboration
TI CHARACTERIZING LOW-MASS BINARIES FROM OBSERVATION OF LONG-TIMESCALE
CAUSTIC-CROSSING GRAVITATIONAL MICROLENSING EVENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; gravitational lensing: micro
ID SOLAR-TYPE STARS; LENS; PHOTOMETRY; SYSTEMS; MULTIPLICITY; RESOLUTION;
ROTATION; DISTANCE; PLANETS; SEARCH
AB Despite the astrophysical importance of binary star systems, detections are limited to those located in small ranges of separations, distances, and masses and thus it is necessary to use a variety of observational techniques for a complete view of stellar multiplicity across a broad range of physical parameters. In this paper, we report the detections and measurements of two binaries discovered from observations of microlensing events MOA-2011-BLG-090 and OGLE-2011-BLG-0417. Determinations of the binary masses are possible by simultaneously measuring the Einstein radius and the lens parallax. The measured masses of the binary components are 0.43M(circle dot) and 0.39M(circle dot) for MOA-2011-BLG-090 and 0.57M(circle dot) and 0.17M(circle dot) for OGLE-2011-BLG-0417 and thus both lens components of MOA-2011-BLG-090 and one component of OGLE-2011-BLG-0417 are M dwarfs, demonstrating the usefulness of microlensing in detecting binaries composed of low-mass components. From modeling of the light curves considering full Keplerian motion of the lens, we also measure the orbital parameters of the binaries. The blended light of OGLE-2011-BLG-0417 comes very likely from the lens itself, making it possible to check the microlensing orbital solution by follow-up radial-velocity observation. For both events, the caustic-crossing parts of the light curves, which are critical for determining the physical lens parameters, were resolved by high-cadence survey observations and thus it is expected that the number of microlensing binaries with measured physical parameters will increase in the future.
C1 [Shin, I. -G.; Han, C.; Choi, J. -Y.; Park, S. -Y.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea.
[Udalski, A.; Szymanski, M. K.; Kubiak, M.; Soszynski, I.; Pietrzynski, G.; Poleski, R.; Ulaczyk, K.; Pietrukowicz, P.; Kozllowski, S.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Gould, A.; Skowron, J.; Penny, M. T.; Batista, V.; Gaudi, B. S.; Henderson, C.; McGregor, D.; Pogge, R. W.; Yee, J. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84081 Baronissi, SA, Italy.
[Bozza, V.; Scarpetta, G.] Sez Napoli, Grp Collegato Salerno, INFN, Naples, Italy.
[Dominik, M.; Horne, K.; Browne, P.; Dodds, P.; Hundertmark, M.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Fouque, P.; Bachelet, E.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France.
[Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Abe, F.; Furusawa, K.; Itow, Y.; Kobara, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Ohmori, K.; Suzuki, K.; Takino, S.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[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, N Shore Mail Ctr, Auckland, New Zealand.
[Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand.
[Chote, P.; Sullivan, D. J.; Tristram, P. J.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand.
[Fukui, A.] NAOJ, Okayama Astrophys Observ, Okayama 7190232, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[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.
[Street, R. A.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Tsapras, Y.] Univ London, Sch Phys & Astron, London E1 4NS, England.
[Alsubai, K. A.] Qatar Fdn, Doha, Qatar.
[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.
[Dreizler, S.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Fang, X. -S.; Gu, C. -H.] Chinese Acad Sci, Joint Lab Opt Astron, Natl Astron Observ, Yunnan Observ, Kunming 650011, Peoples R China.
[Grundahl, F.; Jessen-Hansen, J.; Lund, M.; Lunkkvist, M.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark.
[Hardis, S.; Harpsoe, K.; Hinse, T. C.; Jorgensen, U. G.; Mathiasen, M.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Harpsoe, K.; Jorgensen, U. G.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Hinse, T. C.; Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Hornstrup, A.] Danmarks Tekn Univ, Inst Rumforskning Teknol, DK-2100 Copenhagen, Denmark.
[Kains, N.] ESO Headquarters, D-85748 Garching, Germany.
[Kerins, E.; Penny, M. T.] Univ Manchester, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England.
[Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Rahvar, S.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Ricci, D.; Surdej, J.; Wertz, O.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Southworth, J.; Tregloan-Reed, J.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Wambsganss, J.; Zub, M.] Univ Heidelberg, ZAH, Zentrum Astron, Astronom Rechen Inst, D-69120 Heidelberg, Germany.
[Almeida, L. A.; Jablonski, F.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, SP, Brazil.
[Christie, G.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland, New Zealand.
[DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Dong, Subo] Inst Adv Study, Princeton, NJ 08540 USA.
[McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand.
[Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand.
[Natusch, T.] AUT Univ, Auckland, New Zealand.
[Tan, T. -G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia.
[Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, C.; Kubas, D.; Marquette, J. -B.] Inst Astrophys, UPMC CNRS, UMR 7095, F-75014 Paris, France.
[Brillant, S.; Kubas, D.] European So Observ, Santiago 19, Chile.
[Cole, A. A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia.
[Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria.
[Menzies, J. W.] S African Astron Observ, ZA-7925 Cape Town, South Africa.
[Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
MIT, Dept Phys, Cambridge, MA 02139 USA.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran 9161, Iran.
RP Shin, IG (reprint author), Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea.
RI Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012; Almeida,
L./G-7188-2012; Greenhill, John/C-8367-2013; 7, INCT/H-6207-2013;
Astrofisica, Inct/H-9455-2013; Kozlowski, Szymon/G-4799-2013; Skowron,
Jan/M-5186-2014; Hundertmark, Markus/C-6190-2015; Rahvar,
Sohrab/A-9350-2008
OI Tan, Thiam-Guan/0000-0001-5603-6895; Ricci, Davide/0000-0002-9790-0552;
Penny, Matthew/0000-0001-7506-5640; Snodgrass,
Colin/0000-0001-9328-2905; Lund, Mikkel Norup/0000-0001-9214-5642;
Lundkvist, Mia Sloth/0000-0002-8661-2571; Dominik,
Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855; Kozlowski,
Szymon/0000-0003-4084-880X; Skowron, Jan/0000-0002-2335-1730;
Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725
FU Creative Research Initiative Program of National Research Foundation of
Korea [2009-0081561]; European Research Council under the European
Community [246678]; JSPS [JSPS23540339, JSPS19340058]; German Research
Foundation (DFG); Communaute francaise de Belgique Actions de recherche
concertees-Academie universitaire Wallonie-Europe; Qatar Foundation
through QNRF [NPRP-09-476-1-78]; European Union [268421]; Danish Natural
Science Foundation (FNU); NSF [AST-1103471]; NASA [NNG04GL51G]; National
Science Foundation Graduate Research Fellowship [2009068160]; California
Institute of Technology (Caltech); KRCF Young Scientist Research
Fellowship Program; Korea Astronomy and Space Science Institute (KASI)
[2012-1-410-02]; [JSPS22403003]; [JSPS23340064]; [JSPS23340044]
FX Work by C.H. was supported by Creative Research Initiative Program
(2009-0081561) of National Research Foundation of Korea. 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. The MOA experiment was supported by grants
JSPS22403003 and JSPS23340064. T.S. was supported by the grant
JSPS23340044. Y. Muraki acknowledges support from JSPS grants
JSPS23540339 and JSPS19340058. The MiNDSTEp monitoring campaign is
powered by ARTEMiS (Automated Terrestrial Exoplanet Microlensing Search;
Dominik et al. 2008). M.H. acknowledges support by the German Research
Foundation (DFG). D.R. (boursier FRIA) and J. Surdej acknowledge support
from the Communaute francaise de Belgique Actions de recherche
concertees-Academie universitaire Wallonie-Europe. The RoboNet team is
supported by the Qatar Foundation through QNRF grant NPRP-09-476-1-78.
C.S. received funding from the European Union Seventh Framework
Programme (FPT/2007-2013) under grant agreement 268421. This work is
based in part on data collected by MiNDSTEp with the Danish 1.54 m
telescope at the ESO La Silla Observatory. The Danish 1.54 m telescope
is operated based on a grant from the Danish Natural Science Foundation
(FNU). A. Gould and B.S. Gaudi acknowledge support from NSF AST-1103471.
B. S. Gaudi, A. Gould, and R. W. Pogge acknowledge support from NASA
grant NNG04GL51G. Work by J.C. Yee is supported by a National Science
Foundation Graduate Research Fellowship under grant no. 2009068160. S.
Dong's research was performed under contract with the California
Institute of Technology (Caltech) funded by NASA through the Sagan
Fellowship Program. Research by T.C.H. was carried out under the KRCF
Young Scientist Research Fellowship Program. T.C.H. and C.U.L.
acknowledge the support of Korea Astronomy and Space Science Institute
(KASI) grant 2012-1-410-02.
NR 38
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2012
VL 755
IS 2
AR 91
DI 10.1088/0004-637X/755/2/91
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400008
ER
PT J
AU von Kienlin, A
Gruber, D
Kouveliotou, C
Granot, J
Baring, MG
Gogus, E
Huppenkothen, D
Kaneko, Y
Lin, L
Watts, AL
Bhat, NP
Guiriec, S
van der Horst, AJ
Bissaldi, E
Greiner, J
Meegan, CA
Paciesas, WS
Preece, RD
Rau, A
AF von Kienlin, Andreas
Gruber, David
Kouveliotou, Chryssa
Granot, Jonathan
Baring, Matthew G.
Gogus, Ersin
Huppenkothen, Daniela
Kaneko, Yuki
Lin, Lin
Watts, Anna L.
Bhat, Narayana P.
Guiriec, Sylvain
van der Horst, Alexander J.
Bissaldi, Elisabetta
Greiner, Jochen
Meegan, Charles A.
Paciesas, William S.
Preece, Robert D.
Rau, Arne
TI DETECTION OF SPECTRAL EVOLUTION IN THE BURSTS EMITTED DURING THE
2008-2009 ACTIVE EPISODE OF SGR J1550-5418
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (SGR J1550-5418; 1E 1547.0-5408; PSR J1550-5418);
stars: neutron; X-rays: bursts
ID X-RAY PULSAR; STRONG MAGNETIC-FIELDS; SOFT GAMMA-REPEATERS; 1E
1547.0-5408; STATISTICAL PROPERTIES; TIME-SERIES; MONITOR; EMISSION;
PERIOD; SCATTERING
AB In early 2008 October, the soft gamma repeater SGR J1550-5418 (1E 1547.0-5408, AX J155052-5418, PSR J1550-5418) became active, emitting a series of bursts which triggered the Fermi Gamma-ray Burst Monitor (GBM) after which a second especially intense activity period commenced in 2009 January and a third, less active period was detected in 2009 March-April. Here, we analyze the GBM data for all the bursts from the first and last active episodes. We performed temporal and spectral analysis for all events and found that their temporal characteristics are very similar to the ones of other SGR bursts, as well the ones reported for the bursts of the main episode (average burst durations similar to 170 ms). In addition, we used our sample of bursts to quantify the systematic uncertainties of the GBM location algorithm for soft gamma- ray transients to less than or similar to 8 degrees. Our spectral analysis indicates significant spectral evolution between the first and last set of events. Although the 2008 October events are best fitted with a single blackbody function, for the 2009 bursts an optically thin thermal bremsstrahlung is clearly preferred. We attribute this evolution to changes in the magnetic field topology of the source, possibly due to effects following the very energetic main bursting episode.
C1 [von Kienlin, Andreas; Gruber, David; Bissaldi, Elisabetta; Greiner, Jochen; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Granot, Jonathan] Open Univ Israel, IL-43537 Raanana, Israel.
[Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Gogus, Ersin; Kaneko, Yuki; Lin, Lin] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
[Huppenkothen, Daniela; Watts, Anna L.; van der Horst, Alexander J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Bhat, Narayana P.; Guiriec, Sylvain; Paciesas, William S.; Preece, Robert D.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
[Guiriec, Sylvain] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[van der Horst, Alexander J.; Meegan, Charles A.] NSSTC, Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Bissaldi, Elisabetta] Univ Innsbruck, Inst Astro & Particle Phys, A-6176 Innsbruck, Austria.
RP von Kienlin, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM azk@mpe.mpg.de
RI Bissaldi, Elisabetta/K-7911-2016;
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece,
Robert/0000-0003-1626-7335
FU GBM/Magnetar Key Project (NASA) [NNH07ZDA001-GLAST]; Bundesministerium
fur Bildung und Forschung (BMBF) via the Deutsches Zentrum fur Luft und
Raumfahrt (DLR) [50 QV 0301]; Bundesministeriums fur Wirtschaft und
Technologie (BMWi) through DLR [50 OG 1101]; NASA grant
[NNH07ZDA001GLAST, NNX10AC59A]; Scientific and Technological Research
Council of Turkey (TUBITAK) [109T755]; Post-Doctoral Research Fellowship
of the Turkish Academy of Sciences (TUBA); NWO Vidi grant
FX This publication is part of the GBM/Magnetar Key Project (NASA grant
NNH07ZDA001-GLAST, PI: C. Kouveliotou). Support for the German
contribution to GBM was provided by the Bundesministerium fur Bildung
und Forschung (BMBF) via the Deutsches Zentrum fur Luft und Raumfahrt
(DLR) under contract number 50 QV 0301. A.v.K. was supported by the
Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR
grant 50 OG 1101. C.K. and A.J.v.d.H. were partially supported by NASA
grant NNH07ZDA001GLAST. M.G.B. acknowledges support from NASA through
grant NNX10AC59A. E.G. and Y.K. acknowledge the support from the
Scientific and Technological Research Council of Turkey (TUBITAK)
through grant 109T755. L.L. is supported through the Post-Doctoral
Research Fellowship of the Turkish Academy of Sciences (TUBA). D.H. and
A.L.W. acknowledge support from an NWO Vidi grant (PI: A.L. Watts).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2012
VL 755
IS 2
AR 150
DI 10.1088/0004-637X/755/2/150
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992PL
UT WOS:000307791400067
ER
PT J
AU Currie, T
Fukagawa, M
Thalmann, C
Matsumura, S
Plavchan, P
AF Currie, Thayne
Fukagawa, Misato
Thalmann, Christian
Matsumura, Soko
Plavchan, Peter
TI DIRECT DETECTION AND ORBITAL ANALYSIS OF THE EXOPLANETS HR 8799 bcd FROM
ARCHIVAL 2005 KECK/NIRC2 DATA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; stars: early-type; stars: individual (HR 8799)
ID COMPANION; SYSTEM; PLANET; IMAGE; INCLINATION; STABILITY; DISCOVERY;
DISK; STAR; MASS
AB We present previously unpublished 2005 July H-band coronagraphic data of the young, planet-hosting star HR 8799 from the newly released Keck/NIRC2 archive. Despite poor observing conditions, we detect three of the planets (HR 8799 bcd), two of them (HR 8799 bc) without advanced image processing. Comparing these data with previously published 1998-2011 astrometry and that from re-reduced 2010 October Keck data constrains the orbits of the planets. Analyzing the planets' astrometry separately, HR 8799 d's orbit is likely inclined at least 25 degrees from face-on and the others may be on inclined orbits. For semimajor axis ratios consistent with a 4: 2: 1 mean-motion resonance, our analysis yields precise values for HR 8799 bcd's orbital parameters and strictly constrains the planets' eccentricities to be less than 0.18-0.3. However, we find no acceptable orbital solutions with this resonance that place the planets in face-on orbits; HR 8799 d shows the largest deviation from such orbits. Moreover, few orbits make HR 8799 d coplanar with b and c, whereas dynamical stability analyses used to constrain the planets' masses typically assume coplanar and/or face-on orbits. This Letter illustrates the significant science gain enabled with the release of the NIRC2 archive.
C1 [Currie, Thayne] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Fukagawa, Misato] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka, Japan.
[Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Matsumura, Soko] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Plavchan, Peter] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Currie, T (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
FU National Aeronautics and Space Administration; Astronomy Center for
Theory and Computation Prize Fellowship at the University of Maryland
FX We thank Christian Marois, Scott Kenyon, and the anonymous referee for
helpful comments. This research has made use of the Keck Observatory
Archive (KOA), which is operated by the W. M. Keck Observatory and the
NASA Exoplanet Science Institute (NExScI), under contract with the
National Aeronautics and Space Administration. We are extremely grateful
to the NExScI/KOA staff for developing and maintaining the NIRC2
archive. T.C. is supported by a NASA Postdoctoral Fellowship; S.M. is
supported by an Astronomy Center for Theory and Computation Prize
Fellowship at the University of Maryland.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 20
PY 2012
VL 755
IS 2
AR L34
DI 10.1088/2041-8205/755/2/L34
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 989VM
UT WOS:000307588900012
ER
PT J
AU McDonald, M
Wei, LH
Veilleux, S
AF McDonald, Michael
Wei, Lisa H.
Veilleux, Sylvain
TI COLD MOLECULAR GAS ALONG THE COOLING X-RAY FILAMENT IN A1795
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: clusters: individual (Abell 1795); galaxies:
clusters: intracluster medium; galaxies: elliptical and lenticular, cD;
ISM: jets and outflows; submillimeter: ISM
ID BRIGHTEST CLUSTER GALAXIES; H-ALPHA FILAMENTS; FLOW CLUSTERS; HERSCHEL
OBSERVATIONS; HYDROGEN EMISSION; LUMINOUS CLUSTERS; SPACE-TELESCOPE; NGC
1275; SPECTROSCOPY; CORES
AB We present the results of interferometric observations of the cool core of A1795 at CO(1-0) using the Combined Array for Research in Millimeter-wave Astronomy. In agreement with previous work, we detect a significant amount of cold molecular gas (3.9 +/- 0.4 x 10(9) M-circle dot) in the central similar to 10 kpc. We report the discovery of a substantial clump of cold molecular gas at clustercentric radius of 30 kpc (2.9 +/- 0.4 x 10(9) M-circle dot), coincident in both position and velocity with the warm, ionized filaments. We also place an upper limit on the H-2 mass at the outer edge of the star-forming filament, corresponding to a distance of 60 kpc (<0.9 x 10(9) M-circle dot). We measure a strong gradient in the H alpha/H-2 ratio as a function of radius, suggesting different ionization mechanisms in the nucleus and filaments of A1795. The total mass of cold molecular gas (similar to 7 x 10(9) M-circle dot) is roughly 30% of the classical cooling estimate at the same position, assuming a cooling time of 10(9) yr. Combining the cold molecular gas mass with the UV-derived star formation rate and the warm, ionized gas mass, the spectroscopically derived X-ray cooling rate is fully accounted for and in good agreement with the cooling byproducts over timescales of similar to 10(9) yr. The overall agreement between the cooling rate of the hot intracluster medium and the mass of the cool gas reservoir suggests that, at least in this system, the cooling flow problem stems from a lack of observable cooling in the more diffuse regions at large radii.
C1 [McDonald, Michael] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Wei, Lisa H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wei, Lisa H.] Atmospher & Environm Res, Lexington, MA 02421 USA.
[Veilleux, Sylvain] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mcdonald@space.mit.edu; lisa.wei@cfa.harvard.edu; veilleux@astro.umd.edu
FU NASA [2834-MIT-SAO-4018]; CXO [NAS8-03060]; NSF [AST-0606932, 100958];
Senior NPP Award
FX M.M. was supported by NASA through contract 2834-MIT-SAO-4018, issued by
CXO under contract NAS8-03060. S.V. acknowledges support from NSF
through contracts AST-0606932, 100958, and from a Senior NPP Award held
at the NASA GSFC. CARMA development and operations are supported by NSF
and partner universities. We thank R. Mushotzky and L. Mundy for helpful
discussions. Finally, we thank the anonymous referee for a careful
review, which has greatly improved the final manuscript.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 20
PY 2012
VL 755
IS 2
AR L24
DI 10.1088/2041-8205/755/2/L24
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 989VM
UT WOS:000307588900002
ER
PT J
AU Kaplan, F
Zhao, W
Richards, JT
Wheeler, RM
Guy, CL
Levine, LH
AF Kaplan, Fatma
Zhao, Wei
Richards, Jeffrey T.
Wheeler, Raymond M.
Guy, Charles L.
Levine, Lanfang H.
TI Transcriptional and Metabolic Insights into the Differential
Physiological Responses of Arabidopsis to Optimal and Supraoptimal
Atmospheric CO2
SO PLOS ONE
LA English
DT Article
ID ELEVATED CARBON-DIOXIDE; GENE-EXPRESSION; PHOTOSYNTHETIC ACCLIMATION;
STOMATAL CONDUCTANCE; SIGNAL-TRANSDUCTION; RISING CO2; PLANTS; GROWTH;
SUGAR; THALIANA
AB Background: In tightly closed human habitats such as space stations, locations near volcano vents and closed culture vessels, atmospheric CO2 concentration may be 10 to 20 times greater than Earth's current ambient levels. It is known that super-elevated (SE) CO2 (>1,200 mu mol mol(-1)) induces physiological responses different from that of moderately elevated CO2 (up to 1,200 mu mol mol(-1)), but little is known about the molecular responses of plants to supra-optimal [CO2]. Methodology/Principal Findings: To understand the underlying molecular causes for differential physiological responses, metabolite and transcript profiles were analyzed in aerial tissue of Arabidopsis plants, which were grown under ambient atmospheric CO2 (400 mmol mol(-1)), elevated CO2 (1,200 mmol mol(-1)) and SE CO2 (4,000 mu mol mol(-1)), at two developmental stages early and late vegetative stage. Transcript and metabolite profiling revealed very different responses to elevated versus SE [CO2]. The transcript profiles of SE CO2 treated plants were closer to that of the control. Development stage had a clear effect on plant molecular response to elevated and SE [CO2]. Photosynthetic acclimation in terms of down-regulation of photosynthetic gene expression was observed in response to elevated [CO2], but not that of SE [CO2] providing the first molecular evidence that there appears to be a fundamental disparity in the way plants respond to elevated and SE [CO2]. Although starch accumulation was induced by both elevated and SE [CO2], the increase was less at the late vegetative stage and accompanied by higher soluble sugar content suggesting an increased starch breakdown to meet sink strength resulting from the rapid growth demand. Furthermore, many of the elevated and SE CO2-responsive genes found in the present study are also regulated by plant hormone and stress. Conclusions/Significance: This study provides new insights into plant acclimation to elevated and SE [CO2] during development and how this relates to stress, sugar and hormone signaling.
C1 [Kaplan, Fatma] USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL USA.
[Zhao, Wei] MedImmune LLC, Gaithersburg, MD USA.
[Richards, Jeffrey T.; Levine, Lanfang H.] Enterprise Advisory Serv Inc, QinetiQ N Amer Engn Serv Contract ESC, Sustainable Syst Appl Res, Kennedy Space Ctr, Kennedy Space Ctr, FL USA.
[Wheeler, Raymond M.] NASA, Engn Directorate, Kennedy Space Ctr, Kennedy Space Ctr, FL USA.
[Guy, Charles L.] Univ Florida, Inst Food & Agr Sci, Dept Environm Hort, Plant Mol & Cellular Biol Program, Gainesville, FL 32611 USA.
RP Kaplan, F (reprint author), Res LLC, Gainesville, FL USA.
EM fkaplan@ufl.edu; lanfang.h.levine@nasa.gov
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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 AUG 20
PY 2012
VL 7
IS 8
AR e43583
DI 10.1371/journal.pone.0043583
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 991WJ
UT WOS:000307733800079
PM 22916280
ER
PT J
AU Bera, PP
Lee, TJ
Kokkila, SI
Francisco, JS
AF Bera, Partha P.
Lee, Timothy J.
Kokkila, Sara I.
Francisco, Joseph S.
TI Design strategies to minimize the radiative efficiency of global warming
molecules and a group increment scheme
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kokkila, Sara I.] Stanford Univ, Stanford, CA 94305 USA.
[Francisco, Joseph S.] Purdue Univ, W Lafayette, IN 47907 USA.
EM Partha.P.Bera@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 471-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621803386
ER
PT J
AU Lee, SE
Mastrapa, R
Kress, M
Phillips, C
AF Lee, Sarah E.
Mastrapa, Rachel
Kress, Monika
Phillips, Cynthia
TI Infrared spectroscopy of hydrocarbons diluted in nitrogen ice:
Implications for planetary and astronomy studies
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Lee, Sarah E.] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA.
[Kress, Monika; Phillips, Cynthia] SETI Inst, Mountain View, CA 94043 USA.
[Mastrapa, Rachel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM sarah.lee@students.sjsu.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 220-CHED
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621801731
ER
PT J
AU Liu, YD
Sander, SP
AF Liu, Yingdi
Sander, Stanley P.
TI Low temperatures and pressure dependence study of OH and CO reaction
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Liu, Yingdi; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
EM YINGDI@CALTECH.EDU
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 131-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621807293
ER
PT J
AU Meador, MAB
AF Meador, Mary Ann B.
TI Spacesuits to refrigeration to pipelines: Insulating aerogels
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Meador, Mary Ann B.] NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM maryann.meador@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 5-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621808186
ER
PT J
AU Nguyen, THT
Wilson, MA
Wei, CY
Pohorille, A
AF Nguyen, Thuy Hien T.
Wilson, Michael A.
Wei, Chenyu
Pohorille, Andrew
TI Molecular dynamics studies of small ion channels: Linking structure and
conductance
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Nguyen, Thuy Hien T.] Univ Sci Philadelphia, Dept Chem & Biochem, Philadelphia, PA 19104 USA.
[Wilson, Michael A.; Wei, Chenyu; Pohorille, Andrew] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM tnguyen513@mail.usp.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 382-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621803308
ER
PT J
AU Pilcher, CB
AF Pilcher, Carl B.
TI From nuclear chemistry to astrobiology: How Charles Coryell helped set a
young chemist on a path to exploring life in the universe
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Pilcher, Carl B.] NASA, Ames Res Ctr, Astrobiol Inst, Moffett Field, CA 94035 USA.
EM carl.b.pilcher@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 27-NUCL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621806174
ER
PT J
AU Roberson, LB
AF Roberson, Luke B.
TI International Year of Chemistry closing ceremonies
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Roberson, Luke B.] NASA, Div Mat Sci, Kennedy Space Ctr, FL 32899 USA.
EM Luke.B.Roberson@NASA.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 3-YCC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621808773
ER
PT J
AU Roberson, LB
Canham, S
LaFranzo, N
Dunne, C
AF Roberson, Luke B.
Canham, Stephen
LaFranzo, Natalie
Dunne, Christine
TI 2012 International Conference for Young Chemists
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Roberson, Luke B.] NASA, Div Mat Sci, Kennedy Space Ctr, FL 32899 USA.
EM stephencanham@gmail.com
NR 0
TC 0
Z9 0
U1 1
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 4-YCC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621808774
ER
PT J
AU Roberson, LB
AF Roberson, Luke B.
TI Collaborations with the European Young Chemists Network
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Roberson, Luke B.] NASA, Div Mat Sci, Kennedy Space Ctr, FL 32899 USA.
EM Luke.B.Roberson@NASA.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 1-YCC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621808771
ER
PT J
AU Sherwood, D
Roberson, LB
Diamond, S
Puliga, S
AF Sherwood, Danielle
Roberson, Luke B.
Diamond, Stacy
Puliga, Stephen
TI Collaborations with the European Young Chemists Network part 2
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Roberson, Luke B.] NASA, Div Mat Sci, Kennedy Space Ctr, FL USA.
EM Sherwood.danielle@gmail.com; stacy.diamond@ic.fbi.gov;
stephen.pulga@ic.fbi.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 2-YCC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621808772
ER
PT J
AU Vander Wal, RL
Hunter, GW
Street, KW
Xu, JC
Evans, LJ
Berger, GM
Bryg, VM
AF Vander Wal, Randy L.
Hunter, Gary W.
Street, Kenneth W.
Xu, Jennifer C.
Evans, Laura J.
Berger, Gordon M.
Bryg, Vicky M.
TI Energy engineering at the interface via nanomaterials
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 244th National Fall Meeting of the American-Chemical-Society (ACS)
CY AUG 19-23, 2012
CL Philadelphia, PA
SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc
C1 [Vander Wal, Randy L.] Penn State Univ, John & Willie Leone Family Dept Energy & Mineral, University Pk, PA 16802 USA.
[Vander Wal, Randy L.] Penn State Univ, EMS Energy Inst, University Pk, PA 16802 USA.
[Hunter, Gary W.; Street, Kenneth W.; Xu, Jennifer C.; Evans, Laura J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Berger, Gordon M.; Bryg, Vicky M.] NASA Glenn, Natl Ctr Space Explorat Res, USRA, Cleveland, OH 44135 USA.
EM ruv12@psu.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 19
PY 2012
VL 244
MA 38-ENFL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 220XX
UT WOS:000324621803532
ER
PT J
AU Douglass, AR
Stolarski, RS
Strahan, SE
Oman, LD
AF Douglass, A. R.
Stolarski, R. S.
Strahan, S. E.
Oman, L. D.
TI Understanding differences in upper stratospheric ozone response to
changes in chlorine and temperature as computed using CCMVal-2 models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CHEMISTRY-CLIMATE MODEL; HALOGEN OCCULTATION EXPERIMENT; MIDDLE
ATMOSPHERE; GLOBAL VARIATIONS; TECHNICAL NOTE; MEAN OZONE; TRANSPORT;
PHOTOCHEMISTRY; SIMULATION; TRENDS
AB Projections of future ozone levels are made using models that couple a general circulation model with a representation of atmospheric photochemical processes, allowing interactions among photochemical processes, radiation, and dynamics. Such models are known as coupled chemistry-climate models (CCMs). Although developed from common principles and subject to the same boundary conditions, simulated ozone time series vary among models for scenarios for ozone depleting substances (ODSs) and greenhouse gases. Photochemical processes control the upper stratospheric ozone level, and there is broad agreement among CCMs in that ozone increases as ODSs decrease and temperature decreases due to greenhouse gas increase. There are quantitative differences in the ozone sensitivity to chlorine and temperature. We obtain insight into differences in sensitivity by examining the relationship between the upper stratospheric seasonal cycles of ozone and temperature as produced by fourteen CCMs. All simulations conform to expectation in that ozone is less sensitive to temperature when chlorine levels are highest because chlorine catalyzed loss is nearly independent of temperature. Analysis reveals differences in simulated temperature, ozone and reactive nitrogen that lead to differences in the relative importance of ozone loss processes and are most obvious when chlorine levels are close to background. Differences in the relative importance of loss processes underlie differences in simulated sensitivity of ozone to composition change. This suggests 1) that the multimodel mean is not a best estimate of the sensitivity of upper stratospheric ozone to changes in ODSs and temperature; and 2) that the spread of values is not an appropriate measure of uncertainty.
C1 [Douglass, A. R.] NASA, Atmospher Chem & Dynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stolarski, R. S.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Strahan, S. E.] Univ Space Res Assoc, Columbia, MD USA.
RP Douglass, AR (reprint author), NASA, Atmospher Chem & Dynam Lab, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA.
EM Anne.R.Douglass@nasa.gov
RI Douglass, Anne/D-4655-2012; Oman, Luke/C-2778-2009; Stolarski,
Richard/B-8499-2013
OI Oman, Luke/0000-0002-5487-2598; Stolarski, Richard/0000-0001-8722-4012
FU NASA
FX We acknowledge the modeling groups for making their simulations
available for this analysis; the Chemistry-Climate Model Validation
Activity (CCMVal) for the World Climate Research Programme's
Stratospheric Processes and their Role in Climate (SPARC) project for
organizing and coordinating the model data analysis activity; and the
British Atmospheric Data Center (BADC) for collecting and archiving the
CCMVal model output. This study was supported by the NASA Atmospheric
Chemistry, Modeling and Analysis (ACMAP) and Modeling Analysis and
Prediction (MAP) programs.
NR 60
TC 9
Z9 9
U1 0
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 18
PY 2012
VL 117
AR D16306
DI 10.1029/2012JD017483
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 992CR
UT WOS:000307753600004
ER
PT J
AU Zheng, QA
Holt, B
Li, XF
Liu, XN
Zhao, Q
Yuan, YL
Yang, XF
AF Zheng, Quanan
Holt, Benjamin
Li, Xiaofeng
Liu, Xinan
Zhao, Qing
Yuan, Yeli
Yang, Xiaofeng
TI Deep-water seamount wakes on SEASAT SAR image in the Gulf Stream region
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SYNTHETIC-APERTURE RADAR; UNDERWATER BOTTOM TOPOGRAPHY; OCEAN SURFACE
AB A SEASAT synthetic aperture radar (SAR) image taken over the Gulf Stream region shows streak-like patterns. The physics of their generation and interaction with the Gulf Stream are disputed. This study seeks a convincing interpretation for the SAR imagery patterns. Bathymetric maps show that the sea floor area beneath the streaks is the northeast Hoyt Hills, where isolated seamounts with the heights of 20 to 140 m above the background sea floor are distributed. All the SAR imagery streaks originate from these seamounts and extend downstream. Thus the SAR imagery streaks are interpreted as surface roughness imprints of the seamount wakes. Hydrostatic flow dynamics of the generation of wakes on the lee side of a solid obstacle is used to explain the generation mechanism and internal structure of the seamount wakes. The analysis indicates that boundary conditions and hydrodynamic conditions are favorable for the generation and vertical propagation of the seamount wakes to the upper layer. Citation: Zheng, Q., B. Holt, X. Li, X. Liu, Q. Zhao, Y. Yuan, and X. Yang (2012), Deep-water seamount wakes on SEASAT SAR image in the Gulf Stream region, Geophys. Res. Lett., 39, L16604, doi:10.1029/2012GL052661.
C1 [Zheng, Quanan] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Zheng, Quanan; Yuan, Yeli] SOA, Inst Oceanog 1, Qingdao, Peoples R China.
[Holt, Benjamin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Li, Xiaofeng] NOAA, IMSG, NESDIS, Camp Springs, MD USA.
[Liu, Xinan] Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA.
[Zhao, Qing] E China Normal Univ, Minist Educ, Key Lab Geog Informat Sci, Shanghai 200062, Peoples R China.
[Zhao, Qing] E China Normal Univ, Joint Lab Environm Remote Sensing & Data Assimila, Beijing, Peoples R China.
[Zhao, Qing] Chinese Acad Sci, Ctr Earth Observat & Digital Earth, Beijing, Peoples R China.
[Yang, Xiaofeng] Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing, Peoples R China.
RP Zheng, QA (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, 2423 Comp & Space Sci Bldg, College Pk, MD 20742 USA.
EM quanan@atmos.umd.edu
RI ZHAO, Qing/K-8844-2014; yang, xiaofeng/K-5245-2015; Li,
Xiaofeng/B-6524-2008
OI ZHAO, Qing/0000-0003-3433-9435; yang, xiaofeng/0000-0001-9920-4641; Li,
Xiaofeng/0000-0001-7038-5119
FU US National Science Foundation [0962107]; Academician Foundation of
China; National Aeronautics and Space Administration; Shanghai Science
and Technology Committee Program - Special for EXPO [10DZ0581600];
Shanghai Institute of Urban Ecology and Sustainability [SHUES2011A07]
FX This work is partially supported by US National Science Foundation Award
0962107 and Academician Foundation of China. The views, opinions, and
findings contained in this report are those of the authors and should
not be construed as an official NOAA or U.S. Government position,
policy, or decision. B. H. carried out this work at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. The bathymetric map is
downloaded from www.ngdc.noaa.gov/mgg/bathymetry/. This work is also
supported by Shanghai Science and Technology Committee Program - Special
for EXPO under Grant No.10DZ0581600, and a grant (SHUES2011A07) from
Shanghai Institute of Urban Ecology and Sustainability.
NR 21
TC 4
Z9 5
U1 1
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 17
PY 2012
VL 39
AR L16604
DI 10.1029/2012GL052661
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 991ZI
UT WOS:000307742900002
ER
PT J
AU Kvissel, OK
Orsolini, YJ
Stordal, F
Isaksen, ISA
Santee, ML
AF Kvissel, O-K
Orsolini, Y. J.
Stordal, F.
Isaksen, I. S. A.
Santee, M. L.
TI Formation of stratospheric nitric acid by a hydrated ion cluster
reaction: Implications for the effect of energetic particle
precipitation on the middle atmosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SOLAR-PROTON-EVENTS; WAVE SPECTROSCOPIC MEASUREMENTS; ODIN OBSERVATIONS;
SOUTH-POLE; HNO3; WINTER; N2O5; ENHANCEMENTS; EVOLUTION; OZONE
AB In order to improve our understanding of the effects of energetic particle precipitation on the middle atmosphere and in particular upon the nitrogen family and ozone, we have modeled the chemical and dynamical middle atmosphere response to the introduction of a chemical pathway that produces HNO3 by conversion of N2O5 upon hydrated water clusters H+center dot(H2O)(n). We have used an ensemble of simulations with the National Center for Atmospheric Research (NCAR) Whole-Atmosphere Community Climate Model (WACCM) chemistry-climate model. The chemical pathway alters the internal partitioning of the NOy family during winter months in both hemispheres, and ultimately triggers statistically significant changes in the climatological distributions of constituents including: i) a cold season production and loss of HNO3 and N2O5, respectively, and ii) a cold season decrease and increase in NOx/NOy-ratio and O-3, respectively, in the polar regions of both hemispheres. We see an improved seasonal evolution of modeled HNO3 compared to satellite observations from Microwave Limb Sounder (MLS), albeit not enough HNO3 is produced at high altitudes. Through O-3 changes, both temperature and dynamics are affected, allowing for complex chemical-dynamical feedbacks beyond the cold season when the pathway is active. Hence, we also find a NOx polar increase in spring-to-summer in the southern hemisphere, and in spring in the northern hemisphere. The springtime NOx increase arises from anomalously strong poleward transport associated with a weaker polar vortex. We argue that the weakening of zonal-mean polar winds down to the lower stratosphere, which is statistically significant at the 0.90 level in spring months in the southern hemisphere, is caused by strengthened planetary waves induced by the middle and sub-polar latitude zonal asymmetries in O-3 and short-wave heating.
C1 [Kvissel, O-K; Stordal, F.; Isaksen, I. S. A.] Univ Oslo, Dept Geosci, NO-0315 Oslo, Norway.
[Orsolini, Y. J.] Norwegian Inst Air Res, Kjeller, Norway.
[Santee, M. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Kvissel, OK (reprint author), Univ Oslo, Dept Geosci, NO-0315 Oslo, Norway.
EM o.k.kvissel@geo.uio.no
OI Stordal, Frode/0000-0002-5190-6473
FU Norwegian Research Council NORKLIMA program [178629]; Norwegian Research
School in Climate Dynamics (ResClim); NASA
FX O.K.K., Y.O.R. and F.S. were supported by the Norwegian Research Council
NORKLIMA program (Project Arctic_Lis, project number #178629). O.K.K.
has had a three-week stay at NCAR supported by The Norwegian Research
School in Climate Dynamics (ResClim). Work at the Jet Propulsion
Laboratory, California Institute of Technology, was done under contract
with NASA. The authors would like to acknowledge Varavut Limpasuvan and
Amund Sovde for useful comments.
NR 38
TC 8
Z9 8
U1 3
U2 15
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 17
PY 2012
VL 117
AR D16301
DI 10.1029/2011JD017257
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 992CP
UT WOS:000307753400003
ER
PT J
AU Sahu, LK
Kondo, Y
Moteki, N
Takegawa, N
Zhao, Y
Cubison, MJ
Jimenez, JL
Vay, S
Diskin, GS
Wisthaler, A
Mikoviny, T
Huey, LG
Weinheimer, AJ
Knapp, DJ
AF Sahu, L. K.
Kondo, Y.
Moteki, N.
Takegawa, N.
Zhao, Y.
Cubison, M. J.
Jimenez, J. L.
Vay, S.
Diskin, G. S.
Wisthaler, A.
Mikoviny, T.
Huey, L. G.
Weinheimer, A. J.
Knapp, D. J.
TI Emission characteristics of black carbon in anthropogenic and biomass
burning plumes over California during ARCTAS-CARB 2008
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID POLYCYCLIC AROMATIC-HYDROCARBONS; TRANSFORM INFRARED-SPECTROSCOPY;
IONIZATION MASS-SPECTROMETRY; LASER-INDUCED INCANDESCENCE; AEROSOL
OPTICAL-PROPERTIES; ABSORPTION CROSS-SECTION; SIZE DISTRIBUTIONS;
ELEMENTAL CARBON; MIXING STATE; TRACE GASES
AB The impact of aerosols on regional air quality and climate necessitates improved understanding of their emission and microphysical properties. The size distributions of black carbon (BC) and light scattering particles (LSP) were measured with a single particle soot photometer on board the NASA DC-8 aircraft during the ARCTAS mission 2008. Air sampling was made in the air plumes of both urban and forest fire emissions over California during the CARB (California Air Resources Board) phase of the mission. A total of eleven plumes were identified using SO2 and CH3CN tracers for fossil fuel (FF) combustion and biomass burning (BB), respectively. The enhancements of BC and LSP in BB plumes were significantly higher compared to those in FF plumes. The average mass concentration of BC in BB plumes was more than twice that in FF plumes. Except for the BC/CO ratio, distinct emission ratios of BC/CO2, BC/CH3CN, CH3CN/CO, and CO/CO2 were observed in the plumes from the two sources. Similarly, the microphysical properties of BC and LSP also showed distinct behaviors. The BC count median diameter (CMD) of 115 +/- 5 nm in FF plumes was smaller compared to 141 +/- 9 nm in the BB plumes. BC aerosols were thickly coated in BB plumes, the average shell/core ratios were 1.47 and 1.24 in BB and FF plumes, respectively. In the total mass of submicron aerosols, organic aerosols constituted about 67% in the FF plumes and 84% in BB plumes. The contribution of sulfate was also significant in the FF plumes.
C1 [Sahu, L. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India.
[Kondo, Y.; Moteki, N.] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo 113, Japan.
[Takegawa, N.] Univ Tokyo, Adv Sci & Technol Res Ctr, Tokyo, Japan.
[Zhao, Y.] Univ Calif Davis, Air Qual Res Ctr, Davis, CA 95616 USA.
[Cubison, M. J.; Jimenez, J. L.] Univ Colorado Boulder, Dept Chem & Biochem, Boulder, CO USA.
[Cubison, M. J.; Jimenez, J. L.] Univ Colorado Boulder, CIRES, Boulder, CO USA.
[Vay, S.; Diskin, G. S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Wisthaler, A.; Mikoviny, T.] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria.
[Huey, L. G.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Weinheimer, A. J.; Knapp, D. J.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
RP Sahu, LK (reprint author), Phys Res Lab, Ahmadabad 380009, Gujarat, India.
EM lokesh@prl.res.in
RI Jimenez, Jose/A-5294-2008; Kondo, Yutaka/D-1459-2012
OI Jimenez, Jose/0000-0001-6203-1847;
FU NASA [NNX08AD39G, NNX12AC03G, CARB 08-319, USP-SMD-08-009]; ARCTAS;
Ministry of Education, Culture, Sports, Science, and Technology (MEXT);
Japan Science and Technology Agency (JST); Global Environment Research
Fund of the Japanese Ministry of the Environment [B-083]; DOE
[DE-SC0006035]
FX The ARCTAS mission was supported by NASA. We are indebted to all the
ARCTAS participants for their cooperation and support. Special thanks
are due to the flight and ground crews of the NASA DC-8 aircraft. We
thank M. Osuka for his assistance with the field measurements. P. O.
Wennberg provided the SO2 data used for the present study.
This work was supported in part by the Ministry of Education, Culture,
Sports, Science, and Technology (MEXT); the Strategic International
Cooperative Program of the Japan Science and Technology Agency (JST);
and the Global Environment Research Fund of the Japanese Ministry of the
Environment (B-083). CH3CN measurements were supported by the
Austrian Research Promotion Agency (FFG-ALR) and the Tiroler
Zukunftstiftung, operated with the help and support of M. Graus, A.
Hansel, and T. D. Maerk. M. J. Cubison and J. L. Jimenez were supported
by NASA NNX08AD39G and NNX12AC03G, CARB 08-319, and DOE (BER, ASR
program) DE-SC0006035. Y. Zhao was supported in part by NASA's
Tropospheric Chemistry Program (USP-SMD-08-009).
NR 113
TC 20
Z9 20
U1 4
U2 46
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 17
PY 2012
VL 117
AR D16302
DI 10.1029/2011JD017401
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 992CP
UT WOS:000307753400004
ER
PT J
AU Zimmerman, MI
Jackson, TL
Farrell, WM
Stubbs, TJ
AF Zimmerman, M. I.
Jackson, T. L.
Farrell, W. M.
Stubbs, T. J.
TI Plasma wake simulations and object charging in a shadowed lunar crater
during a solar storm
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID EXPANSION; VACUUM; WIND
AB Within a permanently shadowed lunar crater the horizontal flow of solar wind is obstructed by upstream topography, forming a plasma wake that electrostatically diverts ions toward the crater floor and generates a surface potential that can reach kilovolts. In the present work kinetic plasma simulations are employed to investigate the morphology of a lunar crater wake during passage of a solar storm. Results are cast in terms of leading dimensionless ratios including the ion Mach number, ratio of crater depth to plasma Debye length, peak secondary electron yield, and electron temperature versus electron impact energy at peak secondary yield. This small set of ratios allows generalization to a much wider range of scenarios. The kinetic simulation results are fed forward into an equivalent-circuit model of a roving astronaut. In very low-plasma-current environments triboelectric charging of the astronaut suit becomes effectively perpetual, representing a critical engineering concern for roving within shadowed lunar regions. Finally, simulated ion fluxes are used to explore sputtering and implantation processes within an idealized crater. It is suggested that the physics of plasma miniwakes formed in the vicinity of permanently shadowed topography may play a critical role in modulating the enigmatic spatial distribution of volatiles at the lunar poles.
C1 [Zimmerman, M. I.; Jackson, T. L.; Farrell, W. M.; Stubbs, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zimmerman, M. I.; Jackson, T. L.; Farrell, W. M.; Stubbs, T. J.] NASA, Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA.
[Stubbs, T. J.] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, Catonsville, MD 21228 USA.
RP Zimmerman, MI (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM michael.i.zimmerman@nasa.gov
RI Jackson, Telana/E-9102-2012; Stubbs, Timothy/I-5139-2013; Farrell,
William/I-4865-2013
OI Stubbs, Timothy/0000-0002-5524-645X;
FU NASA; LPROPS [NNX08AN76G]; NASA Lunar Science Institute; DREAM virtual
institute [NNX09AG78A]
FX We gratefully acknowledge the generous allocation of NASA Goddard Space
Flight Center computing resources by Tim McClanahan. This research was
supported by an appointment to the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. The support of LPROPS grant
NNX08AN76G and the NASA Lunar Science Institute and DREAM virtual
institute through grant NNX09AG78A are gratefully acknowledged.
NR 20
TC 9
Z9 9
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD AUG 17
PY 2012
VL 117
AR E00K03
DI 10.1029/2012JE004094
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 991WI
UT WOS:000307733600003
ER
PT J
AU Galley, CR
Leibovich, AK
AF Galley, Chad R.
Leibovich, Adam K.
TI Radiation reaction at 3.5 post-Newtonian order in effective field theory
SO PHYSICAL REVIEW D
LA English
DT Article
ID GRAVITATIONAL-RADIATION; 2-BODY SYSTEMS
AB We derive the radiation reaction forces on a compact binary inspiral through 3.5 order in the post-Newtonian expansion using the effective field theory approach. We utilize a recent formulation of Hamilton's variational principle that rigorously extends the usual Lagrangian and Hamiltonian formalisms to dissipative systems, including the inspiral of a compact binary from the emission of gravitational waves. We find agreement with previous results, which thus provides a non-trivial confirmation of the extended variational principle. The results from this work nearly complete the equations of motion for the generic inspiral of a compact binary with spinning constituents through 3.5 post-Newtonian order, as derived entirely with effective field theory, with only the spin-orbit corrections to the potential at 3.5 post-Newtonian remaining.
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.
RP Galley, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU NASA at the Jet Propulsion Laboratory; National Science Foundation
[PHY-0854782]
FX We thank Ira Rothstein for useful discussions. C. R. G. was supported by
the NASA Postdoctoral Program at the Jet Propulsion Laboratory
administered by Oak Ridge Associated Universities through a contract
with NASA. A. K. L. was supported in part by the National Science
Foundation under Grant No. PHY-0854782.
NR 44
TC 12
Z9 12
U1 0
U2 1
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 AUG 17
PY 2012
VL 86
IS 4
AR 044029
DI 10.1103/PhysRevD.86.044029
PG 10
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 991UN
UT WOS:000307727800005
ER
PT J
AU BastaniNejad, M
Mohamed, MA
Elmustafa, AA
Adderley, P
Clark, J
Covert, S
Hansknecht, J
Hernandez-Garcia, C
Poelker, M
Mammei, R
Surles-Law, K
Williams, P
AF BastaniNejad, M.
Mohamed, Md. Abdullah
Elmustafa, A. A.
Adderley, P.
Clark, J.
Covert, S.
Hansknecht, J.
Hernandez-Garcia, C.
Poelker, M.
Mammei, R.
Surles-Law, K.
Williams, P.
TI Evaluation of niobium as candidate electrode material for dc high
voltage photoelectron guns
SO PHYSICAL REVIEW SPECIAL TOPICS-ACCELERATORS AND BEAMS
LA English
DT Article
ID CARBON NANOTUBE FILMS; FIELD-EMISSION; POLARIZED ELECTRONS; PHOTOCATHODE
GUN
AB The field emission characteristics of niobium electrodes were compared to those of stainless steel electrodes using a DC high voltage field emission test apparatus. A total of eight electrodes were evaluated: two 304 stainless steel electrodes polished to mirrorlike finish with diamond grit and six niobium electrodes (two single-crystal, two large-grain, and two fine-grain) that were chemically polished using a buffered-chemical acid solution. Upon the first application of high voltage, the best large-grain and single-crystal niobium electrodes performed better than the best stainless steel electrodes, exhibiting less field emission at comparable voltage and field strength. In all cases, field emission from electrodes (stainless steel and/or niobium) could be significantly reduced and sometimes completely eliminated, by introducing krypton gas into the vacuum chamber while the electrode was biased at high voltage. Of all the electrodes tested, a large-grain niobium electrode performed the best, exhibiting no measurable field emission (< 10 pA) at 225 kV with 20 mm cathode/anode gap, corresponding to a field strength of 18.7 MV/m.
C1 [BastaniNejad, M.; Mohamed, Md. Abdullah; Elmustafa, A. A.] Old Dominion Univ, Norfolk, VA 23529 USA.
[Adderley, P.; Clark, J.; Covert, S.; Hansknecht, J.; Hernandez-Garcia, C.; Poelker, M.; Mammei, R.; Surles-Law, K.] Thomas Jefferson Natl Accelerator Facil, Newport News, VA 23606 USA.
[Williams, P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP BastaniNejad, M (reprint author), Old Dominion Univ, Norfolk, VA 23529 USA.
FU Jefferson Science Associates under U.S. DOE [DE-AC05-84ER40150]; DOE
Office of High Energy Physics; Americas Region ILC RD program
FX This paper was authored by Jefferson Science Associates under U.S. DOE
Contract No. DE-AC05-84ER40150 and with funding from the DOE Office of
High Energy Physics and the Americas Region ILC R&D program. Thanks to
Peter Kneisel, Larry Turlington, Teena Harris, Scott Williams, and Tom
Elliott of the JLab SRF Institute for extensive help preparing the
niobium electrodes. Thanks to Maria Chetsova for generating the initial
POISSON electrostatic field maps.
NR 37
TC 10
Z9 10
U1 0
U2 7
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-4402
J9 PHYS REV SPEC TOP-AC
JI Phys. Rev. Spec. Top.-Accel. Beams
PD AUG 17
PY 2012
VL 15
IS 8
AR 083502
DI 10.1103/PhysRevSTAB.15.083502
PG 11
WC Physics, Nuclear; Physics, Particles & Fields
SC Physics
GA 992BE
UT WOS:000307749500001
ER
PT J
AU Song, WL
Veca, LM
Kong, CY
Ghose, S
Connell, JW
Wang, P
Cao, L
Lin, Y
Meziani, MJ
Qian, HJ
LeCroy, GE
Sun, YP
AF Song, Wei-Li
Veca, L. Monica
Kong, Chang Yi
Ghose, Sayata
Connell, John W.
Wang, Ping
Cao, Li
Lin, Yi
Meziani, Mohammed J.
Qian, Haijun
LeCroy, Gregory E.
Sun, Ya-Ping
TI Polymeric nanocomposites with graphene sheets - Materials and device for
superior thermal transport properties
SO POLYMER
LA English
DT Article
DE Thermal transport; Polymeric nanocomposite; Graphene sheets
ID WALLED CARBON NANOTUBES; GRAPHITE NANOPLATELET; CONDUCTIVITY;
COMPOSITES; BLENDS; FILMS
AB Polymeric nanocomposites of high thermal conductivities are developed for their significant potential applications in modern electronics, transportation, and space technologies. Among widely studied nanoscale fillers are carbon nanomaterials of superior thermal transport characteristics, whose incorporation into polymeric matrices may result in nanocomposites that exhibit a good combination of processability and thermal conductivity. In this work we prepared specifically exfoliated few-layer graphene nanosheets (GNs), and dispersed them into two different polymeric matrices, the poly(ethylene-vinyl acetate) copolymer (PEVA) and polyimide (PI). The GNs, generally less than 10 nm in thickness according to X-ray and microscopy characterization results, were found to substantially enhance the thermal transport properties in the resulting polymeric nanocomposite films. The same enhancement was also found in the devices fabricated from the nanocomposites, specifically tubes from melt-extrusion, suggesting significant application potentials of the polymeric/GN nanocomposite materials. The ability for the GNs to impart electrical conductivity into the nanocomposite films was also determined, with the results correlated in terms of the percolation theory. The relative enhancement effects of the GNs at different loadings in the nanocomposite films on thermal and electrical transports are highlighted and discussed. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Song, Wei-Li; Veca, L. Monica; Kong, Chang Yi; Wang, Ping; Cao, Li; Lin, Yi; Meziani, Mohammed J.; Qian, Haijun; LeCroy, Gregory E.; Sun, Ya-Ping] Clemson Univ, Dept Chem, Lab Emerging Mat & Technol, Hunter Labs, Clemson, SC 29634 USA.
[Ghose, Sayata; Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Sun, YP (reprint author), Clemson Univ, Dept Chem, Lab Emerging Mat & Technol, Hunter Labs, POB 340973, Clemson, SC 29634 USA.
EM monica.veca@imt.ro; john.w.connell@nasa.gov; syaping@clemson.edu
RI Veca, Lucia/A-4622-2012; Kong, Chang Yi/A-6559-2017
OI Kong, Chang Yi/0000-0001-6465-2006
FU NASA Langley Research Center; China Scholarship Council; Japan Society
for the Promotion of Science (JSPS); Susan G. Komen for the Cure
Postdoctoral Fellowship; South Carolina Space Grant Consortium
FX This work was made possible by financial support from the NASA Langley
Research Center. W.-LS. was a visiting student from School of Materials
Science and Engineering (the group of Prof. Mao-Sheng Cao) at Beijing
Institute of Technology with a fellowship provided by the China
Scholarship Council. C.Y.K. was supported by the Excellent Young
Researchers Overseas Visit Program of Japan Society for the Promotion of
Science (JSPS), L.C. by a Susan G. Komen for the Cure Postdoctoral
Fellowship, and M.J.M. and G.E.L. by the South Carolina Space Grant
Consortium.
NR 29
TC 20
Z9 21
U1 5
U2 108
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0032-3861
EI 1873-2291
J9 POLYMER
JI Polymer
PD AUG 17
PY 2012
VL 53
IS 18
BP 3910
EP 3916
DI 10.1016/j.polymer.2012.07.008
PG 7
WC Polymer Science
SC Polymer Science
GA 990EP
UT WOS:000307614100009
ER
PT J
AU Behrangi, A
Sorooshian, S
Hsu, KL
AF Behrangi, Ali
Sorooshian, Soroosh
Hsu, Kuo-lin
TI Summertime evaluation of REFAME over the Unites States for near
real-time high resolution precipitation estimation
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Precipitation; Remote sensing; Microwave; Hydrology; Real-time; Global;
REFAME
ID COMBINED PASSIVE MICROWAVE; RAINFALL ALGORITHM; ADVECTION; IMAGERY;
SYSTEM
AB Precipitation is the key input for hydrometeorological modeling and applications. In many regions of the world, including populated areas, ground-based measurement of precipitation (whether from radar or rain gauge) is either sparse in time and space or nonexistent. Therefore, high-resolution satellite-based precipitation products are recognized as critical data sources, especially for rapidly-evolving hydrometeorological events such as flash floods which primarily occur during summer/warm seasons. As "proof of concept", a recently proposed algorithm called Rain Estimation using Forward Adjusted-advection of Microwave Estimates (REFAME) and its variation REFAMEgeo are evaluated over the contiguous United States during summers of 2009 and 2011. Both methods are originally designed for near real-time high resolution precipitation estimation from remotely sensed data. High-resolution Q2 (ground radar) precipitation data, in conjunction with two operational near real-time satellite-based precipitation products (PERSIANN, PERSIANN-CCS) are used as evaluation reference and for comparison. The study is performed at half-hour temporal resolution and at a range of spatial resolutions (0.08-, 0.25-, 0.5-, and 1-degree latitude/longitude). The statistical analyses suggest that REFAMEgeo performs favorably among the studied products in terms of capturing both spatial coverage and intensity of precipitation at near real-time with the temporal resolution offered by geostationary satellites. With respect to volume precipitation, REFAMEgeo together with REFAME demonstrates slight overestimation of intense precipitation and underestimation of light precipitation events. Compared to REFAME, It is observed that REFAMEgeo maintains stable performance, even when the amount of accessible microwave (MW) overpasses is limited. Based on the encouraging outcome of this study which was intended as "proof of concept", further testing for other seasons and data-rich regions is the next logical step. Upon confirmation of the relative reliability of the algorithm, it is reasonable to recommend the use of its precipitation estimates for data-sparse regions of the world. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Behrangi, Ali] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sorooshian, Soroosh; Hsu, Kuo-lin] Univ Calif Irvine, Dept Civil & Environm Engn, Henry Samueli Sch Engn, CHRS, Irvine, CA USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-304, Pasadena, CA 91109 USA.
EM ali.behrangi@jpl.nasa.gov; soroosh@uci.edu; kuolinh@uci.edu
RI sorooshian, soroosh/B-3753-2008
OI sorooshian, soroosh/0000-0001-7774-5113
FU NASA-PMM [NNX10AK07G]; NASA NEWS [NNX06AF934]; US Army Research Office
[W911NF-11-1-0422]; National Aeronautics and Space Administration;
California Institute of Technology, Government
FX Partial financial support was provided by the NASA-PMM (Grant
NNX10AK07G), and the NASA NEWS (Grant NNX06AF934), and the US Army
Research Office project (Grant W911NF-11-1-0422). The authors thank Dan
Braithwaite and Eyal Amitai for their technical assistance on processing
the satellite/radar data for this experiment. Part of the research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. (C)2011 California Institute of Technology, Government
sponsorship acknowledged.
NR 26
TC 1
Z9 2
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
J9 J HYDROL
JI J. Hydrol.
PD AUG 16
PY 2012
VL 456
BP 130
EP 138
DI 10.1016/j.jhydrol.2012.06.033
PG 9
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 996BX
UT WOS:000308060100012
ER
PT J
AU Park, J
Moon, YJ
Gopalswamy, N
AF Park, J.
Moon, Y. -J.
Gopalswamy, N.
TI Dependence of solar proton events on their associated activities:
Coronal mass ejection parameters
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ENERGETIC PARTICLE EVENTS; INTERPLANETARY SHOCKS; PREDICTIONS
AB In this study we have examined the occurrence probability of solar proton events (SPEs) and their peak fluxes depending on coronal mass ejection (CME) parameters, linear speed (V), angular width (AW), and location (L). For this we used the NOAA SPE list and their associated CME data from 1997 to 2006. We found that the probability strongly depends on CME speed and angular width as follows. The highest association (36.1%) is found for the full halo CMEs with V >= 1500 kms(-1) but the lowest association (0.9%) is found for the partial halo CMEs with 400 kms(-1) <= V < 1000 kms(-1). The SPE occurrence probabilities are different as much as 4.9 to 23 times according to CME speed and 1.6 to 6.5 times to angular width. The probabilities depending on CME speed and location increase from the eastern region to the western region and with speed. We have also examined the relationship between CME speed and SPE flux as well as its dependence on angular width (partial halo and full halo), longitude (east, center, and west) and direction parameter (<0.4 and >= 0.4). Our results show that the relationships strongly depend on longitude as well as direction parameter.
C1 [Park, J.; Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea.
[Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Moon, YJ (reprint author), Kyung Hee Univ, Sch Space Res, 1 Seocheon Dong, Yongin 446701, South Korea.
EM moonyj@khu.ac.kr
RI Moon, Yong-Jae/E-1711-2013
FU WCU program through the National Research Foundation of Korea
[R31-10016]; Ministry of Education, Science and Technology; Korea
Research Foundation Grant; Korean Government (MOEHRD)
[KRF-2008-314-C00158, 20090071744, 20100014501]; Korea Meteorological
Administration/National Meteorological Satellite Center; NASA's LWS/TRT
program
FX This work has been supported by the WCU program (R31-10016) through the
National Research Foundation of Korea funded by the Ministry of
Education, Science and Technology and by the Korea Research Foundation
Grant funded by the Korean Government (MOEHRD, Basic Research Promotion
Fund) (KRF-2008-314-C00158, 20090071744 and 20100014501). This work is
also supported by the Korea Meteorological Administration/National
Meteorological Satellite Center. NG was supported by NASA's LWS/TRT
program.
NR 27
TC 12
Z9 13
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 16
PY 2012
VL 117
AR A08108
DI 10.1029/2011JA017477
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992CW
UT WOS:000307754100001
ER
PT J
AU McDonald, M
Bayliss, M
Benson, BA
Foley, RJ
Ruel, J
Sullivan, P
Veilleux, S
Aird, KA
Ashby, MLN
Bautz, M
Bazin, G
Bleem, LE
Brodwin, M
Carlstrom, JE
Chang, CL
Cho, HM
Clocchiatti, A
Crawford, TM
Crites, AT
Dehaan, T
Desai, S
Dobbs, MA
Dudley, JP
Egami, E
Forman, WR
Garmire, GP
George, EM
Gladders, MD
Gonzalez, AH
Halverson, NW
Harrington, NL
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Liu, J
Lueker, M
Luong-Van, D
Mantz, A
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Miller, ED
Mocanu, L
Mohr, JJ
Montroy, TE
Murray, SS
Natoli, T
Padin, S
Plagge, T
Pryke, C
Rawle, TD
Reichardt, CL
Rest, A
Rex, M
Ruhl, JE
Saliwanchik, BR
Saro, A
Sayre, JT
Schaffer, KK
Shaw, L
Shirokoff, E
Simcoe, R
Song, J
Spieler, HG
Stalder, B
Staniszewski, Z
Stark, AA
Story, K
Stubbs, CW
Suhada, R
van Engelen, A
Vanderlinde, K
Vieira, JD
Vikhlinin, A
Williamson, R
Zahn, O
Zenteno, A
AF McDonald, M.
Bayliss, M.
Benson, B. A.
Foley, R. J.
Ruel, J.
Sullivan, P.
Veilleux, S.
Aird, K. A.
Ashby, M. L. N.
Bautz, M.
Bazin, G.
Bleem, L. E.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Clocchiatti, A.
Crawford, T. M.
Crites, A. T.
Dehaan, T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Egami, E.
Forman, W. R.
Garmire, G. P.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
Harrington, N. L.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Jones, C.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Liu, J.
Lueker, M.
Luong-Van, D.
Mantz, A.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Miller, E. D.
Mocanu, L.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Natoli, T.
Padin, S.
Plagge, T.
Pryke, C.
Rawle, T. D.
Reichardt, C. L.
Rest, A.
Rex, M.
Ruhl, J. E.
Saliwanchik, B. R.
Saro, A.
Sayre, J. T.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Simcoe, R.
Song, J.
Spieler, H. G.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Story, K.
Stubbs, C. W.
Suhada, R.
van Engelen, A.
Vanderlinde, K.
Vieira, J. D.
Vikhlinin, A.
Williamson, R.
Zahn, O.
Zenteno, A.
TI A massive, cooling-flow-induced starburst in the core of a luminous
cluster of galaxies
SO NATURE
LA English
DT Article
ID ACTIVE GALACTIC NUCLEI; SOUTH-POLE TELESCOPE; H-ALPHA FILAMENTS; X-RAY
SOURCES; GAS; SPECTROSCOPY; EMISSION
AB In the cores of some clusters of galaxies the hot intracluster plasma is dense enough that it should cool radiatively in the cluster's lifetime(1-3), leading to continuous 'cooling flows' of gas sinking towards the cluster centre, yet no such cooling flow has been observed. The low observed star-formation rates(4,5) and cool gas masses(6) for these 'cool-core' clusters suggest that much of the cooling must be offset by feedback to prevent the formation of a runaway cooling flow(7-10). Here we report X-ray, optical and infrared observations of the galaxy cluster SPT-CLJ2344-4243 (ref. 11) at redshift z = 0.596. These observations reveal an exceptionally luminous (8.2 x 10(45) erg s(-1)) galaxy cluster that hosts an extremely strong cooling flow (around 3,820 solar masses a year). Further, the central galaxy in this cluster appears to be experiencing a massive starburst (formation of around 740 solar masses a year), which suggests that the feedback source responsible for preventing runaway cooling in nearby cool-core clusters may not yet be fully established in SPT-CLJ2344-4243. This large starformation rate implies that a significant fraction of the stars in the central galaxy of this cluster may form through accretion of the intracluster medium, rather than (as is currently thought) assembling entirely via mergers.
C1 [McDonald, M.; Sullivan, P.; Bautz, M.; Miller, E. D.; Simcoe, R.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Bayliss, M.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mantz, A.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Foley, R. J.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, S.] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Clocchiatti, A.] Pontificia Univ Catolica, Dept Astron & Astrofis, Santiago, Chile.
[Dehaan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Egami, E.; Marrone, D. P.; Rawle, T. D.; Rex, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Garmire, G. P.; Lueker, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Joy, M.] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Phys Div, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Phys Dept, Cleveland, OH 44106 USA.
[Pryke, C.] Univ Minnesota, Phys Dept, Minneapolis, MN 55455 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schaffer, K. K.] Inst Chicago, Sch Art, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
RP McDonald, M (reprint author), MIT, MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mcdonald@space.mit.edu
RI Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012;
Williamson, Ross/H-1734-2015;
OI Stubbs, Christopher/0000-0003-0347-1724; Williamson,
Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird,
Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169;
Stark, Antony/0000-0002-2718-9996
FU MIT by NASA; National Science Foundation; Kavli Foundation; Moore
Foundation; NSERC; CRC programme; CIfAR; Harvard University by the NSF;
NASA Hubble Fellowship; KICP Fellowship; Alfred P. Sloan Research
Fellowship; BCCP fellowship
FX M.McD. was supported at MIT by NASA through the Chandra X-ray
Observatory. The South Pole Telescope is supported by the National
Science Foundation, with partial support provided by the Kavli
Foundation, and the Moore Foundation. Support for X-ray analysis was
provided by NASA. Work at McGill University is supported by NSERC, the
CRC programme, and CIfAR, and at Harvard University by the NSF. S. V.
acknowledges a Senior NPP Award held at the NASA Goddard Space Flight
Center. R. K. acknowledges a NASA Hubble Fellowship, B. A. B.
acknowledges a KICP Fellowship, M. A. D. acknowledges an Alfred P. Sloan
Research Fellowship, and O.Z. acknowledges a BCCP fellowship.
NR 30
TC 65
Z9 66
U1 2
U2 11
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD AUG 16
PY 2012
VL 488
IS 7411
BP 349
EP 352
DI 10.1038/nature11379
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 988OS
UT WOS:000307501000035
PM 22895340
ER
PT J
AU Yan, Y
Zhang, L
Wang, J
Yang, JY
Fazal, IM
Ahmed, N
Willner, AE
Dolinar, SJ
AF Yan, Yan
Zhang, Lin
Wang, Jian
Yang, Jeng-Yuan
Fazal, Irfan M.
Ahmed, Nisar
Willner, Alan E.
Dolinar, Samuel J.
TI Fiber structure to convert a Gaussian beam to higher-order optical
orbital angular momentum modes
SO OPTICS LETTERS
LA English
DT Article
ID PROPAGATION; GENERATION; LIGHT
AB We propose a fiber structure of a square core and ring refractive index profile that converts an input circular polarized Gaussian mode into optical orbital angular momentum (OAM) modes. By breaking the circular symmetry of the waveguide, the input circularly polarized fundamental mode in the square core can be coupled into the ring region to generate higher-order OAM modes, corresponding to the transference of spin angular momentum and orbital angular momentum. We show, by using simulation, the generation of OAM modes with a topological charge l up to 9 using<10 mm long fiber. The mode purity is above 96.4% and the extinction ratio can be 30 dB. (C) 2012 Optical Society of America
C1 [Yan, Yan; Zhang, Lin; Wang, Jian; Yang, Jeng-Yuan; Fazal, Irfan M.; Ahmed, Nisar; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
[Dolinar, Samuel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yan, Y (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
EM yanyan@usc.edu
RI Zhang, Lin/E-7913-2011
OI Zhang, Lin/0000-0003-0545-1110
FU Defense Advanced Research Project Agency under the InPho program
FX We acknowledge the support of Defense Advanced Research Project Agency
under the InPho program.
NR 18
TC 24
Z9 24
U1 2
U2 42
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
J9 OPT LETT
JI Opt. Lett.
PD AUG 15
PY 2012
VL 37
IS 16
BP 3294
EP 3296
PG 3
WC Optics
SC Optics
GA 994TY
UT WOS:000307956700001
PM 23381235
ER
PT J
AU Safrankova, J
Goncharov, O
Nemecek, Z
Prech, L
Sibeck, DG
AF Safrankova, J.
Goncharov, O.
Nemecek, Z.
Prech, L.
Sibeck, D. G.
TI Asymmetric magnetosphere deformation driven by hot flow anomaly(ies)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EARTHS BOW SHOCK; TANGENTIAL DISCONTINUITY; ANOMALIES; MAGNETOSHEATH
AB We present a case study of a large deformation of the magnetopause on November 26, 2008. The investigation is based on observations of five THEMIS spacecraft located at the dawn flank in the magnetosphere and magnetosheath, on Cluster measurements at the dusk magnetosheath, and is supported by ACE solar wind monitoring. The main revelation of our study is that the interaction of the IMF discontinuity with the bow shock creates either one very elongated hot flow anomaly (HFA) or a pair of them that is (are) simultaneously observed at both flanks. Whereas the dusk HFA is weak and does not cause observable deformation of the magnetopause, the pressure variations connected with the dawn HFA lead to a magnetopause displacement by approximate to 5 R-E outward from its nominal position. This is followed by a rapid inward motion of the magnetopause approximate to 4 R-E inward with respect to the model location. The surface deformation is so large that the outermost THEMIS spacecraft was in the magnetosphere, whereas the spacecraft located 9 R-E inbound entered into the magnetosheath at the same time. The whole event lasted about 5 minutes. Citation: Safrankova, J., O. Goncharov, Z. Nemecek, L. Prech, and D. G. Sibeck (2012), Asymmetric magnetosphere deformation driven by hot flow anomaly(ies), Geophys. Res. Lett., 39, L15107, doi:10.1029/2012GL052636.
C1 [Safrankova, J.; Goncharov, O.; Nemecek, Z.; Prech, L.] Charles Univ Prague, Fac Math & Phys, CR-18000 Prague 8, Czech Republic.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Nemecek, Z (reprint author), Charles Univ Prague, Fac Math & Phys, V Holesovickach 2, CR-18000 Prague 8, Czech Republic.
EM zdenek.nemecek@mff.cuni.cz
FU NASA [NAS5-02099]; Czech Grant Agency [205/09/0112]; Ministry of
Education of the Czech Republic [MSM 0021620860]; Charles University
Grant Agency [GAUK 163810]
FX The authors acknowledge the NASA contract NAS5-02099 and V. Angelopoulos
for use of data from the THEMIS mission. Specifically, C. W. Carlson and
J. P. McFadden for use of ESA data and K. H. Glassmeier, U. Auster, and
W. Baumjohann for the use of FGM data. The present work was partly
supported by the Czech Grant Agency under contract 205/09/0112, and
partly by the research plan MSM 0021620860 that is financed by the
Ministry of Education of the Czech Republic. O.G. thanks the Charles
University Grant Agency (GAUK 163810) for support.
NR 22
TC 4
Z9 4
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 15
PY 2012
VL 39
AR L15107
DI 10.1029/2012GL052636
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 991ZD
UT WOS:000307742200006
ER
PT J
AU Gopalswamy, N
Makela, P
Akiyama, S
Yashiro, S
Xie, H
MacDowall, RJ
Kaiser, ML
AF Gopalswamy, N.
Maekelae, P.
Akiyama, S.
Yashiro, S.
Xie, H.
MacDowall, R. J.
Kaiser, M. L.
TI Radio-loud CMEs from the disk center lacking shocks at 1 AU
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; BURSTS; SPACECRAFT; EVENTS; SUN
AB A coronal mass ejection (CME) associated with a type II burst and originating close to the center of the solar disk typically results in a shock at Earth in 2-3 days and hence can be used to predict shock arrival at Earth. However, a significant fraction (about 28%) of such CMEs producing type II bursts were not associated with shocks at Earth. We examined a set of 21 type II bursts observed by the Wind/WAVES experiment at decameter-hectometric (DH) wavelengths that had CME sources very close to the disk center (within a central meridian distance of 30 degrees), but did not have a shock at Earth. We find that the near-Sun speeds of these CMEs average to similar to 644 km/s, only slightly higher than the average speed of CMEs associated with radio-quiet shocks. However, the fraction of halo CMEs is only similar to 30%, compared to 54% for the radio-quiet shocks and 91% for all radio-loud shocks. We conclude that the disk-center radio-loud CMEs with no shocks at 1 AU are generally of lower energy and they drive shocks only close to the Sun and dissipate before arriving at Earth. There is also evidence for other possible processes that lead to the lack of shock at 1 AU: (i) overtaking CME shocks merge and one observes a single shock at Earth, and (ii) deflection by nearby coronal holes can push the shocks away from the Sun-Earth line, such that Earth misses these shocks. The probability of observing a shock at 1 AU increases rapidly above 60% when the CME speed exceeds 1000 km/s and when the type II bursts propagate to frequencies below 1 MHz.
C1 [Gopalswamy, N.; Maekelae, P.; Akiyama, S.; Yashiro, S.; Xie, H.; MacDowall, R. J.; Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Maekelae, P.; Akiyama, S.; Yashiro, S.; Xie, H.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
RI MacDowall, Robert/D-2773-2012
FU NASA LWS TRT program
FX We thank the SOHO, Wind and ACE science teams for making the shock data
available on line. This research was supported by NASA LWS TR&T program.
SOHO is a project of international cooperation between ESA and NASA.
NR 24
TC 6
Z9 6
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 15
PY 2012
VL 117
AR A08106
DI 10.1029/2012JA017610
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 992CU
UT WOS:000307753900003
ER
PT J
AU Garcia, L
Farquhar, R
Eastman, T
AF Garcia, Leonard
Farquhar, Robert
Eastman, Timothy
TI New Opportunities for a Historic Spacecraft
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
C1 [Garcia, Leonard; Eastman, Timothy] NASA, Wyle Informat Syst, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Farquhar, Robert] KinetX Inc, Space Explorat, Tempe, AZ USA.
RP Garcia, L (reprint author), NASA, Wyle Informat Syst, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM leonard.n.garcia@nasa.gov
NR 0
TC 2
Z9 2
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1539-4956
J9 SPACE WEATHER
JI Space Weather
PD AUG 15
PY 2012
VL 10
AR S08008
DI 10.1029/2008SW000832
PG 2
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 991ZC
UT WOS:000307742100001
ER
PT J
AU Zhou, RJ
Shi, W
Petersen, E
Chavez-Pirson, A
Stephen, M
Peyghambarian, N
AF Zhou, Renjie
Shi, Wei
Petersen, Eliot
Chavez-Pirson, Arturo
Stephen, Mark
Peyghambarian, Nasser
TI Transform-Limited, Injection Seeded, Q-Switched, Ring Cavity Fiber Laser
SO JOURNAL OF LIGHTWAVE TECHNOLOGY
LA English
DT Article
DE Erbium lasers; fiber lasers; tunable lasers; Q-switched laser
AB We report an Er-doped, actively Q-switched, fiber laser, generating transform-limited pulses based on single-frequency fiber laser seeded ring cavity. The output pulsewidth can be tuned from hundreds of nanoseconds to several microseconds by changing the repetition rate or the open time of the electrical pulse trigger. This injection-seeded, Q-switched ring cavity fiber laser can be operated over the whole C-band. In addition, a theoretical model is developed to numerically study the pulse characteristics by changing the acousto-optic modulator transmission as well as several cavity parameters, such as the cavity length and loss. The numerical results are in good agreement with the experimental results.
C1 [Zhou, Renjie; Shi, Wei; Petersen, Eliot; Chavez-Pirson, Arturo; Peyghambarian, Nasser] NP Photon Inc, Tucson, AZ 85747 USA.
[Shi, Wei; Petersen, Eliot; Chavez-Pirson, Arturo; Peyghambarian, Nasser] Univ Arizona, Ctr Opt Sci, Tucson, AZ 85721 USA.
[Stephen, Mark] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhou, RJ (reprint author), Univ Illinois, Dept Elect & Comp Engn, Champaign, IL 61820 USA.
RI Zhou, Renjie /G-9006-2011
OI Zhou, Renjie /0000-0002-4761-6641
FU U.S. NASA [NNX10CA53C]
FX This work was supported by the U.S. NASA through Contract NNX10CA53C.
NR 19
TC 5
Z9 6
U1 2
U2 24
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0733-8724
J9 J LIGHTWAVE TECHNOL
JI J. Lightwave Technol.
PD AUG 15
PY 2012
VL 30
IS 16
BP 2589
EP 2595
DI 10.1109/JLT.2012.2201446
PG 7
WC Engineering, Electrical & Electronic; Optics; Telecommunications
SC Engineering; Optics; Telecommunications
GA 975MR
UT WOS:000306515900004
ER
PT J
AU Kim, HJ
Bae, HB
Park, Y
Lee, K
Choi, SH
AF Kim, Hyun-Jung
Bae, Hyung-Bin
Park, Yeonjoon
Lee, Kunik
Choi, Sang H.
TI Temperature dependence of crystalline SiGe growth on sapphire (0001)
substrates by sputtering
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE Crystal structure; Single-crystal growth; Polycrystalline deposition;
Semiconducting materials
ID SILICON-ON-SAPPHIRE; EPITAXIAL LAYERS; SUPERLATTICES; RELAXATION;
QUALITY; STRAIN; PFETS
AB The temperature dependence of the film morphology and twin structure of SiGe thin films sputtered on sapphire (0001) substrates was characterized using Scanning Electron Microscopy (SEM), with Electron Backscatter Diffraction (EBSD) and cross-sectional Transmission Electron Microscopy (TEM) analysis. It was observed that the type of growth twin formed was different at the two temperatures evaluated, 820 degrees C and 890 degrees C. At the lower temperature, two crystallographic variants rotated from each other by 60 nucleated and propagated (growth twinning). At the higher temperature, the growth twin was suppressed after continuous films were formed and micro-twin lamellae were formed. Consequently, the volume of twins was reduced with the increase in growth temperature and the crystalline morphology was improved. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Kim, Hyun-Jung; Park, Yeonjoon] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Bae, Hyung-Bin] Korea Adv Inst Sci & Technol, Taejon 305701, South Korea.
[Lee, Kunik] Fed Highway Adm, Dept Transportat, Mclean, VA 22101 USA.
[Choi, Sang H.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Kim, HJ (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM Hyunjung.Kim@NASA.Gov
FU NASA Langley Research Center [IA1-1098]; Federal Highway Administration,
Department of Transportation [IA1-1098]
FX This research was supported by the collaborative agreement between NASA
Langley Research Center and Federal Highway Administration, Department
of Transportation under the inter-agency agreement #IA1-1098. The
authors appreciate the assistance of Mr. Tae Woo Lee and Mr. Young Hoon
Ha, FIB/SEM researchers at KAIST, South Korea.
NR 17
TC 3
Z9 3
U1 0
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0248
J9 J CRYST GROWTH
JI J. Cryst. Growth
PD AUG 15
PY 2012
VL 353
IS 1
BP 124
EP 128
DI 10.1016/j.jcrysgro.2012.05.009
PG 5
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA 970EA
UT WOS:000306109700024
ER
PT J
AU Musselman, KN
Molotch, NP
Margulis, SA
Kirchner, PB
Bales, RC
AF Musselman, Keith N.
Molotch, Noah P.
Margulis, Steven A.
Kirchner, Peter B.
Bales, Roger C.
TI Influence of canopy structure and direct beam solar irradiance on
snowmelt rates in a mixed conifer forest
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Forest; Canopy; Snow; SWE ablation; Direct beam transmissivity; Sky view
factor
ID SUB-ALPINE FOREST; LONGWAVE RADIATION; BOREAL FOREST; UNITED-STATES;
MELTING SNOW; LEAF-AREA; ACCUMULATION; COVER; INTERCEPTION; ABLATION
AB Sub-canopy snow ablation rates were measured for three years at forested research plots in the Sierra Nevada, California with a network of 24 automated snow depth sensors and monthly snow density surveys. Snow ablation rates, in mm SWE day(-1), specific to each depth sensor location were estimated as the seasonal maximum SWE divided by the number of days from peak SWE to snow disappearance. Estimates of sub-canopy direct beam solar irradiance and sky view factor (SVF theta) derived from hemispherical photographs were used to explain the spatial distribution of snow ablation rates. Cumulative direct beam irradiance during the observed snowmelt periods explained the most variability in snow ablation rates for the most cloud-free melt season (58% in 2008; 4 cloudy days; at 15 sensor locations snowmelt duration ranged from 39 days to 88 days and direct irradiance ranged from 96 MJ m(-2) to 603 MJ m(-2)) and explained the least ablation variability for the cloudiest melt season of the study (29% in 2009; 23 cloudy days; at 12 sensor locations snowmelt duration ranged from 45 days to 79 days and direct irradiance ranged from 121 MJ m(-2) to 410 MJ m(-2)). Conversely, sky view factor (SVF theta) explained the most variability in snow ablation rates under cloudier conditions (i.e. 87% in 2009) and the relationships were strongest when developed over the entire hemisphere (i.e. SVF90 degrees, which ranged from 0.17 to 0.31). Combined, the two metrics studied here (sub-canopy direct beam irradiance and SVF theta) may be used to explain much of the observed plot-scale variability in SWE ablation at finer time scales relevant to snow and hydrological model applications. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Musselman, Keith N.; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Musselman, Keith N.; Margulis, Steven A.] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA 90095 USA.
[Musselman, Keith N.; Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kirchner, Peter B.; Bales, Roger C.] Univ Calif, Sierra Nevada Res Inst, Merced, CA 95343 USA.
RP Musselman, KN (reprint author), Univ Colorado, Inst Arctic & Alpine Res, 1560 30th St,450 UCB, Boulder, CO 80309 USA.
EM musselman1@ucla.edu
RI Molotch, Noah/C-8576-2009
FU National Science Foundation [EAR-071160, EAR-1032295, EAR-1032308];
Southern Sierra Critical Zone Observatory [EAR-0725097, EAR-0619947];
Mountain Research Initiative; National Aeronautics and Space
Administration (NASA)
FX The authors thank Sequoia National Park for access rights and continued
support of ongoing research efforts. Financial support was provided by
the National Science Foundation grants EAR-071160, EAR-1032295,
EAR-1032308, the Southern Sierra Critical Zone Observatory
(EAR-0725097), a Major Research Instrumentation grant (EAR-0619947), the
Mountain Research Initiative, and a National Aeronautics and Space
Administration (NASA) Earth System Science Fellowship. J. Melack and J.
Sickman provided valuable solar radiation data from the Tokopah basin.
The authors are grateful to everyone who provided assistance in the
field and office including: B. Forman, D. Perrot, S. Roberts, D.
Berisford, E. Trujillo, L. Meromy, M. Girotto, and M. Cooper, among many
others.
NR 51
TC 29
Z9 29
U1 2
U2 35
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD AUG 15
PY 2012
VL 161
BP 46
EP 56
DI 10.1016/j.agrformet.2012.03.011
PG 11
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 953CH
UT WOS:000304844000004
ER
PT J
AU Gordon, KL
Kang, JH
Park, C
Lillehei, PT
Harrison, JS
AF Gordon, Keith L.
Kang, Jin Ho
Park, Cheol
Lillehei, Peter T.
Harrison, Joycelyn S.
TI A novel negative dielectric constant material based on phosphoric acid
doped poly(benzimidazole)
SO JOURNAL OF APPLIED POLYMER SCIENCE
LA English
DT Article
DE high performance polymers; polymer synthesis and characterization;
dielectric properties; metamaterials; resonance frequency
ID POLYMER ELECTROLYTE; EXPERIMENTAL-VERIFICATION; TRANSMISSION-LINES; ION
OSCILLATIONS; POLYBENZIMIDAZOLE; METAMATERIALS; INDEX; CONDUCTIVITY;
FREQUENCIES; COMPOSITES
AB Metamaterials or artificial negative index materials (NIMs) have generated great attention because of their unique electromagnetic properties. The main challenge in current NIM development is creating a homogenous NIM without the need of complex geometric architectures consisting of capacitors and inductors or aggregated fillers, but possessing a tunable plasma frequency. A natural material that can exhibit negative values for permittivity and permeability simultaneously has not been found, or discovered. If one can design a negative dielectric constant material with a tunable plasma frequency of interest, implementing negative permeability into the material or system would be much more readily achievable to create a metamaterial. In this regard, a novel negative dielectric constant material, which is an essential key to creating the NIMs, was developed by doping ions into a polymer, a protonated poly(benzimidazole) (PBI). The doped PBI showed a negative dielectric constant at frequencies of kHz to MHz because of its reduced plasma frequency and an induction effect. As temperature increased, the dielectric spectrum changed from a relaxation to a resonance behavior and exhibited a larger magnitude of negative dielectric constant at a lower frequency. The conductivity of the doped PBI measured as a function of both temperature and frequency followed the same trend as the dielectric constant. With respect to the dielectric constant and the conductivity data, it can be assumed that the origin of the negative dielectric constant is attributed to the resonance behavior of the highly mobile ions at elevated temperatures and high frequencies. (C) 2012 Wiley Periodicals, Inc. J Appl Polym Sci, 2012
C1 [Kang, Jin Ho; Park, Cheol] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Gordon, Keith L.; Lillehei, Peter T.; Harrison, Joycelyn S.] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
[Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
RP Kang, JH (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA.
EM jin.h.kang@nasa.gov
RI Lillehei, Peter/C-9196-2009
OI Lillehei, Peter/0000-0001-8183-9980
NR 28
TC 8
Z9 8
U1 0
U2 20
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0021-8995
J9 J APPL POLYM SCI
JI J. Appl. Polym. Sci.
PD AUG 15
PY 2012
VL 125
IS 4
BP 2977
EP 2985
DI 10.1002/app.36248
PG 9
WC Polymer Science
SC Polymer Science
GA 936ND
UT WOS:000303596200059
ER
PT J
AU Lee, JE
Risi, C
Fung, I
Worden, J
Scheepmaker, RA
Lintner, B
Frankenberg, C
AF Lee, Jung-Eun
Risi, Camille
Fung, Inez
Worden, John
Scheepmaker, Remco A.
Lintner, Benjamin
Frankenberg, Christian
TI Asian monsoon hydrometeorology from TES and SCIAMACHY water vapor
isotope measurements and LMDZ simulations: Implications for speleothem
climate record interpretation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TIBETAN PLATEAU; CIRCULATION MODEL; LATE MIOCENE; PRECIPITATION;
DELTA-O-18; PALEOCLIMATE; EVAPORATION; CONVECTION; SPACE; ICE
AB Observations show that heavy oxygen isotope composition in precipitation (delta O-18(p)) increases from coastal southeastern (SE) China to interior northwestern (NW) China during the wet season, contradicting expectations from simple Rayleigh distillation theory. Here we employ stable isotopes of precipitation and vapor from satellite measurements and climate model simulations to characterize the moisture processes that control Asian monsoon precipitation and relate these processes to speleothem paleoclimate records. We find that delta O-18(p) is low over SE China as a result of local and upstream condensation and that delta O-18(p) is high over NW China because of evaporative enrichment of O-18 as raindrops fall through dry air. We show that delta O-18(p) at cave sites over southern China is weakly correlated with upstream precipitation in the core of the Indian monsoon region rather than local precipitation, but it is well-correlated with the delta O-18(p) over large areas of southern and central China, consistent with coherent speleothem delta O-18(p) variations over different parts of China. Previous studies have documented high correlations between speleothem delta O-18(p) and millennial timescale climate forcings, and we suggest that the high correlation between insolation and speleothem delta O-18(p) in southern China reflects the variations of hydrologic processes over the Indian monsoon region on millennial and orbital timescales. The delta O-18(p) in the drier part (north of similar to 30 degrees N) of China, on the other hand, has consistently negative correlations with local precipitation and may capture local hydrologic processes related to changes in the extent of the Hadley circulation.
C1 [Lee, Jung-Eun; Worden, John; Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Risi, Camille] CNRS, LMD, IPSL, Paris, France.
[Fung, Inez] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Scheepmaker, Remco A.] SRON Netherlands Inst Space Res, SRON, Utrecht, Netherlands.
[Lintner, Benjamin] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA.
RP Lee, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-200, Pasadena, CA 91109 USA.
EM jung-eun.lee@jpl.nasa.gov
RI Frankenberg, Christian/A-2944-2013
OI Frankenberg, Christian/0000-0002-0546-5857
FU National Aeronautics and Space Administration; NASA ROSES
[NNH07ZDA001N-AST 07-AST07-0069, NNH07ZDA001N-NEWS 07-NEWS07-0020];
National Science Foundation [EAR-090919]; National Science Foundation
Paleo Perspectives on Climate Change [AGS-1103209]; Netherlands Space
Office as part of the User Support Programme Space Research project
[GO-AO/16]
FX We thank D. Battisti and R. L. Edwards for helpful discussions, and we
also thank three anonymous reviewers and the Editor (S. Ghan) for
helpful comments on our manuscript. The work described here was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contracts from the National Aeronautics and Space
Administration. The NASA ROSES Aura Science Team NNH07ZDA001N-AST
07-AST07-0069 and NASA ROSES NNH07ZDA001N-NEWS 07-NEWS07-0020
contributed to the support of the analysis. I. F. acknowledges support
by National Science Foundation grant EAR-090919, and B. R. L.
acknowledges support by National Science Foundation Paleo Perspectives
on Climate Change grant AGS-1103209. LMDZ simulations were performed on
the NEC-SX6 machine of the IDRIS computing center. R. S. acknowledges
support from the Netherlands Space Office as part of the User Support
Programme Space Research project GO-AO/16.
NR 45
TC 43
Z9 44
U1 3
U2 31
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 14
PY 2012
VL 117
AR D15112
DI 10.1029/2011JD017133
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 992CK
UT WOS:000307752900001
ER
PT J
AU Prikryl, P
Jayachandran, PT
Mushini, SC
Richardson, IG
AF Prikryl, P.
Jayachandran, P. T.
Mushini, S. C.
Richardson, I. G.
TI Toward the probabilistic forecasting of high-latitude GPS phase
scintillation
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID COROTATING INTERACTION REGIONS; CORONAL MASS EJECTIONS; SOLAR-WIND;
IONOSPHERIC SCINTILLATIONS; GEOMAGNETIC STORMS; EXTRATROPICAL CYCLONES;
EQUATORIAL IONOSPHERE; SEMIANNUAL VARIATION; STREAM INTERFACES; MODEL
AB The phase scintillation index was obtained from L1 GPS data collected with the Canadian High Arctic Ionospheric Network (CHAIN) during years of extended solar minimum 2008-2010. Phase scintillation occurs predominantly on the dayside in the cusp and in the nightside auroral oval. We set forth a probabilistic forecast method of phase scintillation in the cusp based on the arrival time of either solar wind corotating interaction regions (CIRs) or interplanetary coronal mass ejections (ICMEs). CIRs on the leading edge of high-speed streams (HSS) from coronal holes are known to cause recurrent geomagnetic and ionospheric disturbances that can be forecast one or several solar rotations in advance. Superposed epoch analysis of phase scintillation occurrence showed a sharp increase in scintillation occurrence just after the arrival of high-speed solar wind and a peak associated with weak to moderate CMEs during the solar minimum. Cumulative probability distribution functions for the phase scintillation occurrence in the cusp are obtained from statistical data for days before and after CIR and ICME arrivals. The probability curves are also specified for low and high (below and above median) values of various solar wind plasma parameters. The initial results are used to demonstrate a forecasting technique on two example periods of CIRs and ICMEs.
C1 [Prikryl, P.] Commun Res Ctr Canada, Ottawa, ON K2H 8S2, Canada.
[Jayachandran, P. T.; Mushini, S. C.] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada.
[Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Richardson, I. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Prikryl, P (reprint author), Commun Res Ctr Canada, Ottawa, ON K2H 8S2, Canada.
EM paul.prikryl@crc.gc.ca
OI Richardson, Ian/0000-0002-3855-3634
FU Canada Foundation for Innovation; New Brunswick Innovation Foundation
FX Infrastructure funding for CHAIN was provided by the Canada Foundation
for Innovation and the New Brunswick Innovation Foundation. CHAIN
operation is conducted in collaboration with the Canadian Space Agency
(CSA). The solar wind data were obtained from Goddard Space Flight
Center Space Physics Data Facility OMNIWeb
(http://omniweb.gsfc.nasa.gov/).
NR 77
TC 13
Z9 13
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1539-4956
J9 SPACE WEATHER
JI Space Weather
PD AUG 14
PY 2012
VL 10
AR S08005
DI 10.1029/2012SW000800
PG 16
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 991YV
UT WOS:000307741300001
ER
PT J
AU Galli, S
Bartlett, JG
Melchiorri, A
AF Galli, Silvia
Bartlett, James G.
Melchiorri, Alessandro
TI Optimizing observational strategy for future f(gas) constraints
SO PHYSICAL REVIEW D
LA English
DT Article
ID GAS MASS FRACTION; RAY GALAXY CLUSTERS; X-RAY; DARK ENERGY; SCALING
RELATIONS; BARYON FRACTION; COSMOLOGY; PARAMETERS; TELESCOPE; PROBE
AB The Planck cluster catalog is expected to contain of order one thousand galaxy clusters, both newly discovered and previously known, detected through the Sunyaev-Zeldovich effect over the redshift range 0 less than or similar to z less than or similar to 1. Follow-up x-ray observations of a dynamically relaxed subsample of newly discovered Planck clusters will improve constraints on the dark energy equation of state found through measurement of the cluster gas mass fraction (f(gas)). In view of follow-up campaigns with XMM-Newton and Chandra satellites, we determine the optimal redshift distribution of a cluster sample to most tightly constrain the dark energy equation of state. The distribution is nontrivial even for the standard w(0)-w(a) parametrization. We then determine how much the combination of expected data from the Planck satellite and f(gas) data will be able to constrain the dark energy equation of state. Our analysis employs a Markov Chain Monte Carlo method as well as a Fisher Matrix analysis. With a suitably large program of observational time to observe only hot relaxed clusters, we find that these upcoming data would be able to improve the figure of merit by at least a factor two.
C1 [Galli, Silvia; Bartlett, James G.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Observ Paris, Paris 13, France.
[Galli, Silvia; Melchiorri, Alessandro] Univ Roma La Sapienza, Ist Nazl Fis Nucl, I-00185 Rome, Italy.
[Galli, Silvia; Melchiorri, Alessandro] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Galli, Silvia] Univ Paris 06, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Galli, Silvia] CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Bartlett, James G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Galli, S (reprint author), Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Observ Paris, 10 Rue Alice Domon & Leonie Duquet, Paris 13, France.
FU Institut Universitaire de France; PRIN-INAF
FX S. G. would like to thank D. Rapetti, B. Wandelt and S. Allen for useful
discussions. A portion of the research described in this paper was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. J. G. B. gratefully acknowledges support from the
Institut Universitaire de France. This work was supported by the
PRIN-INAF grant "Astronomy probes fundamental physics."
NR 51
TC 1
Z9 1
U1 1
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 14
PY 2012
VL 86
IS 4
AR 043516
DI 10.1103/PhysRevD.86.043516
PG 13
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 988PO
UT WOS:000307503200002
ER
PT J
AU Przekop, A
Guo, XY
Rizzi, SA
AF Przekop, Adam
Guo, Xinyun
Rizzi, Stephen A.
TI Alternative modal basis selection procedures for reduced-order nonlinear
random response simulation
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID SMOOTH ORTHOGONAL DECOMPOSITION; VIBRATION; IDENTIFICATION; SYSTEMS;
MODES
AB Three procedures to guide selection of an efficient modal basis in a non meat random response analysis are examined. One method is based only on proper orthogonal decomposition, while the other two additionally involve smooth orthogonal decomposition. Acoustic random response problems are employed to assess the performance of the three modal basis selection approaches. A thermally post-buckled beam exhibiting snap-through behavior, a shallowly curved arch in the auto-parametric response regime and a plate structure are used as numerical test articles. The results of a computationally taxing full-order analysis in physical degrees of freedom are taken as the benchmark for comparison with the results from the three reduced-order analyses. For the cases considered, all three methods are shown to produce modal bases resulting in accurate and computationally efficient reduced-order nonlinear simulations. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Przekop, Adam] Analyt Serv & Mat Inc, Hampton, VA 23666 USA.
[Guo, Xinyun] Daniel Webster Coll, Sch Engn & Comp Sci, Nashua, NH 03063 USA.
[Rizzi, Stephen A.] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA.
RP Przekop, A (reprint author), Analyt Serv & Mat Inc, 107 Res Dr, Hampton, VA 23666 USA.
EM Adam.Przekop@nasa.gov; Guo_David@dwc.edu; Stephen.A.Rizzi@nasa.gov
NR 20
TC 4
Z9 4
U1 0
U2 7
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 AUG 13
PY 2012
VL 331
IS 17
BP 4005
EP 4024
DI 10.1016/j.jsv.2012.03.034
PG 20
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA 956OC
UT WOS:000305098000006
ER
PT J
AU Zhang, CX
Wang, YQ
Lauer, A
Hamilton, K
Xie, FQ
AF Zhang, Chunxi
Wang, Yuqing
Lauer, Axel
Hamilton, Kevin
Xie, Feiqin
TI Cloud base and top heights in the Hawaiian region determined with
satellite and ground-based measurements
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ATMOSPHERIC BOUNDARY-LAYER; CLIMATE-CHANGE; EAST MAUI; OCCULTATION;
MISSION
AB We present a multi-year climatology of cloud-base-height (CBH), cloud-top-height (CTH), and trade wind inversion base height (TWIBH) for the Hawaiian region (18 degrees N-22.5 degrees N, 153.7 degrees W-160.7 degrees W). The new climatology is based on data from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite (CALIPSO), the Constellation Observing System for Meteorology Ionosphere and Climate (COSMIC), ceilometer observations and radiosondes. The climatology reported here is well suited to evaluate climate model simulations and can serve as a reference state for studies of the impact of climate change on Hawaiian ecosystems. The averaged CBH from CALIPSO in the Hawaiian Region is 890 m. The mean CTH from CALIPSO is 2110 m, which is close to the mean TWIBH from COSMIC. For non-precipitating cases, the mean TWIBH at both Lihue and Hilo is close to 2000 m. For precipitating cases, the mean TWIBH is 2450 m and 2280 m at Hilo and Lihue, respectively. The potential cloud thickness (PCT) is defined as the difference between TWIBH and CBH and the mean PCT is several hundred meters thicker for precipitating than for the non-precipitating cases at both stations. We find that the PCT is more strongly correlated to the TWIBH than the CBH and that precipitation is unlikely to occur if the TWIBH is below 1500 m. The observed rainfall intensity is correlated to the PCT, i.e., thicker clouds are more likely to produce heavy rain. Citation: Zhang, C., Y. Wang, A. Lauer, K. Hamilton, and F. Xie (2012), Cloud base and top heights in the Hawaiian region determined with satellite and ground-based measurements, Geophys. Res. Lett., 39, L15706, doi: 10.1029/2012GL052355.
C1 [Zhang, Chunxi; Wang, Yuqing; Lauer, Axel; Hamilton, Kevin] Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA.
[Zhang, Chunxi; Wang, Yuqing; Lauer, Axel; Hamilton, Kevin] Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA.
[Xie, Feiqin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Xie, Feiqin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Wang, YQ (reprint author), Univ Hawaii Manoa, Int Pacific Res Ctr, 1680 East West Rd, Honolulu, HI 96822 USA.
EM yuqing@hawaii.edu
RI XIE, FEIQIN/J-4569-2013;
OI Xie, Feiqin/0000-0002-3936-9759
FU NOAA [NA07OAR4310257, NA09OAR4320075]; DOE Regional and Global Climate
Modeling (RCGM) Program [ER64840]; Japan Agency for Marine-Earth Science
and Technology (JAMSTEC); NASA [NNX07AG53G]
FX This study was supported by NOAA grant NA07OAR4310257 and DOE Regional
and Global Climate Modeling (RCGM) Program grant ER64840. Additional
support was provided by the Japan Agency for Marine-Earth Science and
Technology (JAMSTEC), by NASA through grant NNX07AG53G, and by NOAA
through grant NA09OAR4320075, which sponsor research at the
International Pacific Research Center. We would like to acknowledge
NCDC, NASA Langley Research Center, UCAR COSMIC program, and the
University of Wyoming for making their data publicly available.
NR 21
TC 6
Z9 6
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 11
PY 2012
VL 39
AR L15706
DI 10.1029/2012GL052355
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 988BV
UT WOS:000307464100003
ER
PT J
AU Tian, BJ
Ao, CO
Waliser, DE
Fetzer, EJ
Mannucci, AJ
Teixeira, J
AF Tian, Baijun
Ao, Chi O.
Waliser, Duane E.
Fetzer, Eric J.
Mannucci, Anthony J.
Teixeira, Joao
TI Intraseasonal temperature variability in the upper troposphere and lower
stratosphere from the GPS radio occultation measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; MOIST THERMODYNAMIC STRUCTURE; TRANSITION
LAYER CIRRUS; TROPICAL TROPOPAUSE; SAC-C; VERTICAL STRUCTURE;
WATER-VAPOR; ATMOSPHERE; CHAMP; MJO
AB In this study, we examine the detailed spatiotemporal patterns and vertical structure of the intraseasonal temperature variability in the upper troposphere and lower stratosphere (UTLS) associated with the Madden-Julian Oscillation (MJO) using the temperature profiles from the recent Global Positioning System radio occultation (GPS RO) measurements including the Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) mission. The MJO-related temperature anomalies in the UTLS are smaller near the equator (<0.6 K) than over the subtropics and extratropics (>1.2 K). Near the equator, the temperature anomalies exhibit an eastward tilt with height from the upper troposphere (UT) to the lower stratosphere (LS) and their magnitudes and signs are determined by the strength of convective anomalies and vertical pressure level. The subtropical temperature anomalies have similar magnitudes and patterns at a given location between the UT (250 hPa to 150 hPa) and the LS (150 hPa to 50 hPa) except for opposite signs that change around 150 hPa. The subtropical warm (cold) anomalies in the UT and cold (warm) anomalies in the LS are typically collocated with the subtropical positive (negative) tropopause height anomalies/cyclones (anticyclones) and flank or lie to the west of equatorial enhanced (suppressed) convection. We also compare the intraseasonal temperature variability in the UTLS related to the MJO between the GPS RO and Atmospheric Infrared Sounder (AIRS) measurements to highlight the new features of the GPS RO temperature anomalies and to evaluate the quality of the AIRS temperature in the UTLS considering the GPS RO temperature in the UTLS as the benchmark. Both AIRS and GPS RO have a very consistent vertical structure in the subtropical UTLS with a high correlation coefficient 0.92 and similar magnitudes. Both AIRS and GPS RO also show a generally consistent vertical structure of the intraseasonal temperature anomalies in the equatorial UTLS. However, GPS RO reveals many detailed fine-scale vertical structures of the equatorial temperature anomalies between 150 and 50 hPa that are not well captured by AIRS. Furthermore, the equatorial temperature anomalies are about 40% underestimated in AIRS in comparison to GPS RO, over the equatorial Indian and western Pacific Oceans for 250 hPa and over all longitudes for 100 hPa. The low sampling within the optically thick clouds and low vertical resolution near the tropopause may both contribute to these deficiencies of AIRS.
C1 [Tian, Baijun; Ao, Chi O.; Waliser, Duane E.; Fetzer, Eric J.; Mannucci, Anthony J.; Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tian, BJ (reprint author), CALTECH, Jet Prop Lab, M-S 233-304,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM baijun.tian@jpl.nasa.gov
RI Tian, Baijun/A-1141-2007
OI Tian, Baijun/0000-0001-9369-2373
FU National Aeronautics and Space Administration (NASA); Research and
Technology Development program; Atmospheric Infrared Sounder (AIRS)
project at JPL
FX This research was performed at Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), under a contract with
National Aeronautics and Space Administration (NASA). It was supported
jointly by the Research and Technology Development program and
Atmospheric Infrared Sounder (AIRS) project at JPL. We thank three
anonymous reviewers for their constructive comments that helped improve
the quality of this paper.
NR 67
TC 8
Z9 8
U1 0
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 11
PY 2012
VL 117
AR D15110
DI 10.1029/2012JD017715
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 988AS
UT WOS:000307461100003
ER
PT J
AU Jaggard, V
Turyshev, SG
AF Jaggard, Victoria
Turyshev, Slava G.
TI One minute with ... Slava G. Turyshev
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [Turyshev, Slava G.] NASA, Jet Prop Lab, Pasadena, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD AUG 11
PY 2012
VL 215
IS 2877
BP 27
EP 27
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 988LZ
UT WOS:000307493800018
ER
PT J
AU Jahn, A
Aksenov, Y
de Cuevas, BA
de Steur, L
Hakkinen, S
Hansen, E
Herbaut, C
Houssais, MN
Karcher, M
Kauker, F
Lique, C
Nguyen, A
Pemberton, P
Worthen, D
Zhang, J
AF Jahn, A.
Aksenov, Y.
de Cuevas, B. A.
de Steur, L.
Hakkinen, S.
Hansen, E.
Herbaut, C.
Houssais, M. -N.
Karcher, M.
Kauker, F.
Lique, C.
Nguyen, A.
Pemberton, P.
Worthen, D.
Zhang, J.
TI Arctic Ocean freshwater: How robust are model simulations?
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; SEA-ICE DYNAMICS; THERMOHALINE CIRCULATION;
NARES STRAIT; NUMERICAL INVESTIGATIONS; THICKNESS DISTRIBUTION; SEASONAL
VARIABILITY; THERMODYNAMIC MODEL; LANCASTER SOUND; FRAM STRAIT
AB The Arctic freshwater (FW) has been the focus of many modeling studies, due to the potential impact of Arctic FW on the deep water formation in the North Atlantic. A comparison of the hindcasts from ten ocean-sea ice models shows that the simulation of the Arctic FW budget is quite different in the investigated models. While they agree on the general sink and source terms of the Arctic FW budget, the long-term means as well as the variability of the FW export vary among models. The best model-to-model agreement is found for the interannual and seasonal variability of the solid FW export and the solid FW storage, which also agree well with observations. For the interannual and seasonal variability of the liquid FW export, the agreement among models is better for the Canadian Arctic Archipelago (CAA) than for Fram Strait. The reason for this is that models are more consistent in simulating volume flux anomalies than salinity anomalies and volume-flux anomalies dominate the liquid FW export variability in the CAA but not in Fram Strait. The seasonal cycle of the liquid FW export generally shows a better agreement among models than the interannual variability, and compared to observations the models capture the seasonality of the liquid FW export rather well. In order to improve future simulations of the Arctic FW budget, the simulation of the salinity field needs to be improved, so that model results on the variability of the liquid FW export and storage become more robust. Citation: Jahn, A., et al. (2012), Arctic Ocean freshwater: How robust are model simulations?, J. Geophys. Res., 117, C00D16, doi: 10.1029/2012JC007907.
C1 [Jahn, A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Aksenov, Y.; de Cuevas, B. A.] Natl Oceanog Ctr Southampton, Southampton, Hants, England.
[de Steur, L.] NIOZ Royal Netherlands Inst Sea Res, Den Burg, Netherlands.
[Hakkinen, S.; Worthen, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hansen, E.] Norwegian Polar Res Inst, Tromso, Norway.
[Herbaut, C.; Houssais, M. -N.] Univ Paris 06, UMR CNRS UPMC IRD MNHN, LOCEAN, Paris, France.
[Karcher, M.; Kauker, F.] Alfred Wegener Inst Polar & Marine Res, Bremerhaven, Germany.
[Lique, C.] Univ Washington, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA.
[Nguyen, A.] MIT, Cambridge, MA 02139 USA.
[Pemberton, P.] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden.
[Pemberton, P.] Swedish Meteorol & Hydrol Inst, Oceanog Res Unit, S-60176 Norrkoping, Sweden.
[Worthen, D.] Wyle Informat Syst Grp, Mclean, VA USA.
[Zhang, J.] Univ Washington, Coll Ocean & Fishery Sci, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
RP Jahn, A (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM ajahn@ucar.edu
RI Jahn, Alexandra/C-6545-2008; Lique, Camille/L-5543-2015;
OI Jahn, Alexandra/0000-0002-6580-2579; Lique, Camille/0000-0002-8357-4928;
de Steur, Laura/0000-0002-6043-7920
FU National Science Foundation Office of Polar Programs [ARC-0804010];
Advanced Study Program at the National Center for Atmospheric Research
(NCAR); National Science Foundation; UK Natural Environment Research
Council; project "Advanced Simulation of Arctic climate change and
impact on Northern regions" (ADSIMNOR) [214-2009-389]; Swedish Research
Council for Environment, Agricultural Sciences and Spatial Planning
(FORMAS); NSF [ARC-0901987, ARC-0908769]; European Community FP7 through
the THOR project [GA212643]; German Federal Ministry for Education and
Research, BMBF
FX The manuscript was inspired by discussions at the annual Arctic Ocean
Model Intercomparison Project (AOMIP) workshops, and we are thankful to
AOMIP (funded by the National Science Foundation Office of Polar
Programs, award ARC-0804010) for travel support to attend AOMIP meetings
and for covering the publications fees. We thank all AOMIP participants
for the discussions and feedback that helped to shape and improve the
work presented in this manuscript, and especially Rudiger Gerdes (AWI)
and Cornelia Koberle (AWI) for discussions of the initial design of the
study, as well as Andrey Proshutinsky (WHOI) for acting as editor. We
also want to thank Humfrey Melling for discussions about the mooring
data from Nares Strait and Simon Prinsenberg for sharing the FW fluxes
calculated from the moorings in Lancaster Sound with us and for feedback
on the manuscript. Comments from Marika Holland also helped to improve
an earlier version of the manuscript and are much appreciated. We also
thank two anonymous reviewers for their constructive and detailed
comments that helped us to further improve the manuscript. Alexandra
Jahn was supported through a Postdoctoral Fellowship from the Advanced
Study Program at the National Center for Atmospheric Research (NCAR).
NCAR is sponsored by the National Science Foundation. The POP2-CICE
simulation was performed by S. Yaeger (NCAR) as part of the CORE-II suit
of simulations, using CISL computer resources. At the National
Oceanography Centre (NOC) Southampton (Yevgeny Aksenov and Beverly de
Cuevas) this study was funded by the UK Natural Environment Research
Council as a contribution to the Marine Centres' Strategic Research
Programme Oceans2025. NOC also acknowledges the use of UK National High
Performance Computing Resource. Per Pemberton was supported by the
project "Advanced Simulation of Arctic climate change and impact on
Northern regions" (ADSIMNOR, 214-2009-389) funded by the Swedish
Research Council for Environment, Agricultural Sciences and Spatial
Planning (FORMAS). Jinlun Zhang was supported by NSF (grants ARC-0901987
and ARC-0908769) during his contribution to this manuscript. The ORCA025
simulation has been carried out within the DRAKKAR project, and was run
at the IDRIS CNRS-GENCI computer center in Orsay, France, by J.M.
Molines. Work performed at LOCEAN was partly supported by the European
Community FP7 through the THOR project under grant agreement GA212643.
Computing resources have been provided by the French "Institut du
Developpement et des Ressources en Informatique Scientifique" (IDRIS).
M. Karcher and F. Kauker are grateful for funding support from the
project "The North Atlantic as Part of the Earth System: From System
Comprehension to Analysis of Regional Impacts" from the German Federal
Ministry for Education and Research, BMBF.
NR 109
TC 27
Z9 27
U1 0
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD AUG 10
PY 2012
VL 117
AR C00D16
DI 10.1029/2012JC007907
PG 22
WC Oceanography
SC Oceanography
GA 095PW
UT WOS:000315347800001
ER
PT J
AU Bonaca, A
Tanner, JD
Basu, S
Chaplin, WJ
Metcalfe, TS
Monteiro, MJPFG
Ballot, J
Bedding, TR
Bonanno, A
Broomhall, AM
Bruntt, H
Campante, TL
Christensen-Dalsgaard, J
Corsaro, E
Elsworth, Y
Garcia, RA
Hekker, S
Karoff, C
Kjeldsen, H
Mathur, S
Regulo, C
Roxburgh, I
Stello, D
Trampedach, R
Barclay, T
Burke, CJ
Caldwell, DA
AF Bonaca, Ana
Tanner, Joel D.
Basu, Sarbani
Chaplin, William J.
Metcalfe, Travis S.
Monteiro, Mario J. P. F. G.
Ballot, Jerome
Bedding, Timothy R.
Bonanno, Alfio
Broomhall, Anne-Marie
Bruntt, Hans
Campante, Tiago L.
Christensen-Dalsgaard, Jorgen
Corsaro, Enrico
Elsworth, Yvonne
Garcia, Rafael A.
Hekker, Saskia
Karoff, Christoffer
Kjeldsen, Hans
Mathur, Savita
Regulo, Clara
Roxburgh, Ian
Stello, Dennis
Trampedach, Regner
Barclay, Thomas
Burke, Christopher J.
Caldwell, Douglas A.
TI CALIBRATING CONVECTIVE PROPERTIES OF SOLAR-LIKE STARS IN THE KEPLER
FIELD OF VIEW
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: fundamental parameters; stars: interiors; stars: oscillations
ID MIXING-LENGTH PARAMETER; ALPHA-CENTAURI; ASTEROSEISMIC ANALYSIS; HELIUM
ABUNDANCE; INPUT CATALOG; STELLAR AGES; EVOLUTION; OSCILLATIONS; MASS;
ISOCHRONES
AB Stellar models generally use simple parameterizations to treat convection. The most widely used parameterization is the so-called mixing-length theory where the convective eddy sizes are described using a single number, alpha, the mixing-length parameter. This is a free parameter, and the general practice is to calibrate alpha using the known properties of the Sun and apply that to all stars. Using data from NASA's Kepler mission we show that using the solar-calibrated alpha is not always appropriate, and that in many cases it would lead to estimates of initial helium abundances that are lower than the primordial helium abundance. Kepler data allow us to calibrate alpha for many other stars and we show that for the sample of stars we have studied, the mixing-length parameter is generally lower than the solar value. We studied the correlation between alpha and stellar properties, and we find that alpha increases with metallicity. We therefore conclude that results obtained by fitting stellar models or by using population-synthesis models constructed with solar values of alpha are likely to have large systematic errors. Our results also confirm theoretical expectations that the mixing-length parameter should vary with stellar properties.
C1 [Bonaca, Ana; Tanner, Joel D.; Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Basu, Sarbani; Chaplin, William J.; Metcalfe, Travis S.; Christensen-Dalsgaard, Jorgen; Garcia, Rafael A.; Mathur, Savita] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Chaplin, William J.; Broomhall, Anne-Marie; Elsworth, Yvonne] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Metcalfe, Travis S.; Mathur, Savita] NCAR, High Altitude Observ, Boulder, CO 80301 USA.
[Monteiro, Mario J. P. F. G.; Campante, Tiago L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Monteiro, Mario J. P. F. G.; Campante, Tiago L.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
[Ballot, Jerome] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Ballot, Jerome] Univ Toulouse, UPS, IRAP, OMP, F-31400 Toulouse, France.
[Bedding, Timothy R.; Corsaro, Enrico; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Bonanno, Alfio] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy.
[Bruntt, Hans; Christensen-Dalsgaard, Jorgen; Karoff, Christoffer; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Garcia, Rafael A.] Univ Paris Diderot, Lab AIM, Ctr Saclay, CEA DSM,CNRS,IRFU SAp, F-91191 Gif Sur Yvette, France.
[Garcia, Rafael A.] Ctr Etud Saclay, IRFU SAp, F-91191 Gif Sur Yvette, France.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Regulo, Clara] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Regulo, Clara] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain.
[Roxburgh, Ian] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England.
[Trampedach, Regner] Univ Colorado, JILA, Boulder, CO 80309 USA.
[Trampedach, Regner] NIST, Boulder, CO 80309 USA.
[Barclay, Thomas] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Burke, Christopher J.; Caldwell, Douglas A.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Bonaca, A (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA.
EM ana.bonaca@yale.edu; joel.tanner@yale.edu; sarbani.basu@yale.edu
RI Bonanno, Alfio/J-1845-2012; Ballot, Jerome/G-1019-2010; Monteiro, Mario
J.P.F.G./B-4715-2008; Caldwell, Douglas/L-7911-2014;
OI Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776;
Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Caldwell,
Douglas/0000-0003-1963-9616; Bonanno, Alfio/0000-0003-3175-9776;
Bedding, Timothy/0000-0001-5943-1460; Metcalfe,
Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965
FU NASA's Science Mission Directorate; NSF [AST-1105930]; NASA [NNX09AJ53G]
FX We thank the anonymous referee for comments that have improved this
Letter. Funding for the Kepler mission is provided by NASA's Science
Mission Directorate. This work was partially supported by NSF grant
AST-1105930 and NASA grant NNX09AJ53G. We also thank all other funding
councils and agencies that have supported the activities of Working
Group 1 of the Kepler Asteroseismic Science Consortium.
NR 49
TC 31
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2012
VL 755
IS 1
AR L12
DI 10.1088/2041-8205/755/1/L12
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980YS
UT WOS:000306930700012
ER
PT J
AU Deck, KM
Holman, MJ
Agol, E
Carter, JA
Lissauer, JJ
Ragozzine, D
Winn, JN
AF Deck, Katherine M.
Holman, Matthew J.
Agol, Eric
Carter, Joshua A.
Lissauer, Jack J.
Ragozzine, Darin
Winn, Joshua N.
TI RAPID DYNAMICAL CHAOS IN AN EXOPLANETARY SYSTEM
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE celestial mechanics; planets and satellites: dynamical evolution and
stability
ID OUTER ASTEROID BELT; N-BODY PROBLEM; SYMPLECTIC MAPS; 3-BODY PROBLEM;
SOLAR-SYSTEM; SUPER-EARTHS; STABILITY; PROMETHEUS; BEHAVIOR; PANDORA
AB We report on the long-term dynamical evolution of the two-planet Kepler-36 system, which consists of a super-Earth and a sub-Neptune in a tightly packed orbital configuration. The orbits of the planets, which we studied through numerical integrations of initial conditions that are consistent with observations of the system, are chaotic with a Lyapunov time of only similar to 10 years. The chaos is a consequence of a particular set of orbital resonances, with the inner planet orbiting 34 times for every 29 orbits of the outer planet. The rapidity of the chaos is due to the interaction of the 29: 34 resonance with the nearby first-order 6: 7 resonance, in contrast to the usual case in which secular terms in the Hamiltonian play a dominant role. Only one contiguous region of phase space, accounting for similar to 4.5% of the sample of initial conditions studied, corresponds to planetary orbits that do not show large-scale orbital instabilities on the timescale of our integrations (similar to 200 million years). Restricting the orbits to this long-lived region allows a refinement of estimates of the masses and radii of the planets. We find that the long-lived region consists of the initial conditions that satisfy the Hill stability criterion by the largest margin. Any successful theory for the formation of this system will need to account for why its current state is so close to unstable regions of phase space.
C1 [Deck, Katherine M.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Deck, Katherine M.; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Holman, Matthew J.; Carter, Joshua A.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Deck, KM (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
RI Carter, Joshua/A-8280-2013; Agol, Eric/B-8775-2013; Ragozzine,
Darin/C-4926-2013;
OI Agol, Eric/0000-0002-0802-9145; Carter, Joshua/0000-0001-8152-2561
FU NSF [AST-0645416]
FX We thank J. Wisdom for sharing with us his code that calculates
coefficients in the disturbing function, as well as other members of the
Kepler TTV team and our anonymous reviewer for helpful comments on the
text. E. A. acknowledges support for this work which was provided by NSF
Career grant AST-0645416.
NR 29
TC 21
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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 AUG 10
PY 2012
VL 755
IS 1
AR L21
DI 10.1088/2041-8205/755/1/L21
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980YS
UT WOS:000306930700021
ER
PT J
AU Tinker, JL
George, MR
Leauthaud, A
Bundy, K
Finoguenov, A
Massey, R
Rhodes, J
Wechsler, RH
AF Tinker, Jeremy L.
George, Matthew R.
Leauthaud, Alexie
Bundy, Kevin
Finoguenov, Alexis
Massey, Richard
Rhodes, Jason
Wechsler, Risa H.
TI THE CORRELATED FORMATION HISTORIES OF MASSIVE GALAXIES AND THEIR DARK
MATTER HALOS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: groups: general; galaxies: halos
ID DIGITAL SKY SURVEY; FIELD GALAXIES; STAR-FORMATION; ASSEMBLY BIAS;
STELLAR MASS; EVOLUTION; COSMOS; ENVIRONMENT; OCCUPATION; LUMINOSITY
AB Using observations in the COSMOS field, we report an intriguing correlation between the star formation activity of massive (similar to 10(11.4) M-circle dot) central galaxies, their stellar masses, and the large-scale (similar to 10 Mpc) environments of their group-mass (similar to 10(13.6) M-circle dot) dark matter halos. Probing the redshift range z = [0.2, 1.0], our measurements come from two independent sources: an X-ray-detected group catalog and constraints on the stellar-to-halo mass relation derived from a combination of clustering and weak lensing statistics. At z = 1, we find that the stellar mass in star-forming (SF) centrals is a factor of two less than in passive centrals at the same halo mass. This implies that the presence or lack of star formation in group-scale centrals cannot be a stochastic process. By z = 0, the offset reverses, probably as a result of the different growth rates of these objects. A similar but weaker trend is observed when dividing the sample by morphology rather than star formation. Remarkably, we find that SF centrals at z similar to 1 live in groups that are significantly more clustered on 10 Mpc scales than similar mass groups hosting passive centrals. We discuss this signal in the context of halo assembly and recent simulations, suggesting that SF centrals prefer halos with higher angular momentum and/or formation histories with more recent growth; such halos are known to evolve in denser large-scale environments. If confirmed, this would be evidence of an early established link between the assembly history of halos on large scales and the future properties of the galaxies that form inside them.
C1 [Tinker, Jeremy L.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Leauthaud, Alexie; Bundy, Kevin] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Finoguenov, Alexis] Max Planck Inst Expt Phys, D-85748 Garchingbei Munchen, Germany.
[Massey, Richard] Univ Maryland, Inst Computat, Baltimore, MD 21250 USA.
[Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA.
[Wechsler, Risa H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Wechsler, Risa H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Wechsler, Risa H.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
RP Tinker, JL (reprint author), NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
EM jeremy.tinker@nyu.edu
FU World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan; NASA [HST-GO-09822]; JPL
FX We thank Charlie Conroy and Tom Theuns for useful discussions. This work
was supported by World Premier International Research Center Initiative
(WPI Initiative), MEXT, Japan. The initial HST-COSMOS Treasury program
was supported through NASA grant HST-GO-09822. We gratefully acknowledge
contributions of the entire COSMOS collaboration consisting of more than
140 scientists. More information on COSMOS is available at
http://cosmos.astro.caltech.edu/ and the data archive is at IPAC/IRSA.
J.R. was supported by JPL, run under contract for NASA by Caltech.
NR 32
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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 AUG 10
PY 2012
VL 755
IS 1
AR L5
DI 10.1088/2041-8205/755/1/L5
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980YS
UT WOS:000306930700005
ER
PT J
AU Faryabi, H
Davami, K
Kheirabi, N
Shaygan, M
Lee, JS
Meyyappan, M
AF Faryabi, Hamid
Davami, Keivan
Kheirabi, Nazli
Shaygan, Mehrdad
Lee, Jeong-Soo
Meyyappan, M.
TI Post-growth modification of electrical properties of ZnTe nanowires
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID THIN-FILMS; OPTICAL-PROPERTIES; ROUTE
AB ZnTe nanowires, grown by a vapor-liquid-solid technique are p-type and show a very high intrinsic resistivity. Enhancement of the nanowire conductivity was investigated by vacuum annealing, doping and Joule heating. The current-voltage (I-V) characteristics were measured in all cases and electrical parameters such as resistivity, carrier concentration and mobility were computed from the I-V curves. An improvement of five orders of magnitude in the electrical conductivity was seen after thermal annealing and Joule heating, comparable to the enhancement in conductivity obtained by doping. Published by Elsevier B.V.
C1 [Faryabi, Hamid; Davami, Keivan; Kheirabi, Nazli; Shaygan, Mehrdad; Lee, Jeong-Soo; Meyyappan, M.] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 790894, South Korea.
RP Meyyappan, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM lj56951@postech.ac.kr; m.meyyappan@nasa.gov
FU World Class University program; Ministry of Education, Science and
Technology through the National Research Foundation of Korea [R31-10100]
FX This research was supported by the World Class University program funded
by the Ministry of Education, Science and Technology through the
National Research Foundation of Korea (R31-10100).
NR 25
TC 6
Z9 6
U1 3
U2 30
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD AUG 10
PY 2012
VL 543
BP 117
EP 120
DI 10.1016/j.cplett.2012.06.052
PG 4
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 981ML
UT WOS:000306972300022
ER
PT J
AU Abadie, J
Abbott, BP
Abbott, TD
Abbott, R
Abernathy, M
Adams, C
Adhikari, R
Affeldt, C
Ajith, P
Allen, B
Allen, GS
Ceron, EA
Amariutei, D
Amin, RS
Anderson, SB
Anderson, WG
Arai, K
Arain, MA
Araya, MC
Aston, SM
Atkinson, D
Aufmuth, P
Aulbert, C
Aylott, BE
Babak, S
Baker, P
Ballmer, S
Barker, D
Barnum, S
Barr, B
Barriga, P
Barsotti, L
Barton, MA
Bartos, I
Bassiri, R
Bastarrika, M
Bauchrowitz, J
Behnke, B
Bell, AS
Belopolski, I
Benacquista, M
Bertolini, A
Betzwieser, J
Beveridge, N
Beyersdorf, PT
Bilenko, IA
Billingsley, G
Birch, J
Biswas, R
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Bland, B
Bock, O
Bodiya, TP
Bogan, C
Bondarescu, R
Bork, R
Born, M
Bose, S
Boyle, M
Brady, PR
Braginsky, VB
Brau, JE
Breyer, J
Bridges, DO
Brinkmann, M
Britzger, M
Brooks, AF
Brown, DA
Brummitt, A
Buonanno, A
Burguet-Castell, J
Burmeister, O
Byer, RL
Cadonati, L
Camp, JB
Campsie, P
Cannizzo, J
Cannon, K
Cao, J
Capano, C
Caride, S
Caudill, S
Cavaglia, M
Cepeda, C
Chalermsongsak, T
Chalkley, E
Charlton, P
Chelkowski, S
Chen, Y
Christensen, N
Chua, SSY
Chung, S
Chung, CTY
Clara, F
Clark, D
Clark, J
Clayton, JH
Conte, R
Cook, D
Corbitt, TRC
Cornish, N
Costa, CA
Coughlin, M
Coward, DM
Coyne, DC
Creighton, JDE
Creighton, TD
Cruise, AM
Cumming, A
Cunningham, L
Culter, RM
Dahl, K
Danilishin, SL
Dannenberg, R
Danzmann, K
Das, K
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Fazi, D
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Finn, LS
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Foley, S
Forsi, E
Fotopoulos, N
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Friedrich, D
Fritschel, P
Frolov, VV
Fulda, P
Fyffe, M
Garcia, J
Garofoli, JA
Gholami, I
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Gill, C
Goetz, E
Goggin, LM
Gonzalez, G
Gorodetsky, ML
Gossler, S
Graef, C
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Grosso, R
Grote, H
Grunewald, S
Guido, C
Gupta, R
Gustafson, EK
Gustafson, R
Hage, B
Hallam, JM
Hammer, D
Hammond, G
Hanks, J
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Heefner, J
Hendry, MA
Heng, IS
Heptonstall, AW
Herrera, V
Hewitson, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Hong, T
Hooper, S
Hosken, DJ
Hough, J
Howell, EJ
Hughey, B
Husa, S
Huttner, SH
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Johnson, WW
Jones, DI
Jones, G
Jones, R
Ju, L
Kalmus, P
Kalogera, V
Kandhasamy, S
Kanner, JB
Katsavounidis, E
Katzman, W
Kawabe, K
Kawamura, S
Kawazoe, F
Kells, W
Kelner, M
Keppel, DG
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, N
Kim, H
King, PJ
Kinzel, DL
Kissel, JS
Klimenko, S
Kondrashov, V
Kopparapu, R
Koranda, S
Korth, WZ
Kozak, D
Kringel, V
Krishnamurthy, S
Krishnan, B
Kuehn, G
Kumar, R
Kwee, P
Landry, M
Lantz, B
Lastzka, N
Lazzarini, A
Leaci, P
Leong, J
Leonor, I
Li, J
Lindquist, PE
Lockerbie, NA
Lodhia, D
Lormand, M
Lu, P
Luan, J
Lubinski, M
Luck, H
Lundgren, AP
Macdonald, E
Machenschalk, B
MacInnis, M
Mageswaran, M
Mailand, K
Mandel, I
Mandic, V
Marandi, A
Marka, S
Marka, Z
Maros, E
Martin, IW
Martin, RM
Marx, JN
Mason, K
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McIver, J
McKechan, DJA
Meadors, G
Mehmet, M
Meier, T
Melatos, A
Melissinos, AC
Mendell, G
Mercer, RA
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Miller, J
Mino, Y
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Moe, B
Moesta, P
Mohanty, SD
Moraru, D
Moreno, G
Mossavi, K
Mow-Lowry, CM
Mueller, G
Mukherjee, S
Mullavey, A
Muller-Ebhardt, H
Munch, J
Murphy, D
Murray, PG
Nash, T
Nawrodt, R
Nelson, J
Newton, G
Nishizawa, A
Nolting, D
Nuttall, L
O'Reilly, B
O'Shaughnessy, R
Ochsner, E
O'Dell, J
Ogin, GH
Oldenburg, RG
Osthelder, C
Ott, CD
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Page, A
Pan, Y
Pankow, C
Papa, MA
Patel, P
Pedraza, M
Pekowsky, L
Penn, S
Peralta, C
Perreca, A
Phelps, M
Pickenpack, M
Pinto, IM
Pitkin, M
Pletsch, HJ
Plissi, MV
Podkaminer, J
Pold, J
Postiglione, F
Predoi, V
Price, LR
Prijatelj, M
Principe, M
Privitera, S
Prix, R
Prokhorov, L
Puncken, O
Quetschke, V
Raab, FJ
Radkins, H
Raffai, P
Rakhmanov, M
Ramet, CR
Rankins, B
Mohapatra, SRP
Raymond, V
Redwine, K
Reed, CM
Reed, T
Reid, S
Reitze, DH
Riesen, R
Riles, K
Roberts, P
Robertson, NA
Robinson, C
Robinson, EL
Roddy, S
Rollins, J
Romano, JD
Romie, JH
Rover, C
Rowan, S
Rudiger, A
Ryan, K
Sakata, S
Sakosky, M
Salemi, F
Salit, M
Sammut, L
de la Jordana, LS
Sandberg, V
Sannibale, V
Santamaria, L
Santiago-Prieto, I
Santostasi, G
Saraf, S
Sathyaprakash, BS
Sato, S
Saulson, PR
Savage, R
Schilling, R
Schlamminger, S
Schnabel, R
Schofield, RMS
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Searle, AC
Seifert, F
Sellers, D
Sengupta, AS
Sergeev, A
Shaddock, DA
Shaltev, M
Shapiro, B
Shawhan, P
Weerathunga, TS
Shoemaker, DH
Sibley, A
Siemens, X
Sigg, D
Singer, A
Singer, L
Sintes, AM
Skelton, G
Slagmolen, BJJ
Slutsky, J
Smith, R
Smith, JR
Smith, MR
Smith, ND
Somiya, K
Sorazu, B
Soto, J
Speirits, FC
Stein, AJ
Steinlechner, J
Steinlechner, S
Steplewski, S
Stefszky, M
Stochino, A
Stone, R
Strain, KA
Strigin, S
Stroeer, AS
Stuver, AL
Summerscales, TZ
Sung, M
Susmithan, S
Sutton, PJ
Szokoly, GP
Talukder, D
Tanner, DB
Tarabrin, SP
Taylor, JR
Taylor, R
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Thuring, A
Tokmakov, KV
Torres, C
Torrie, CI
Traylor, G
Trias, M
Tseng, K
Ugolini, D
Urbanek, K
Vahlbruch, H
Vaishnav, B
Vallisneri, M
Van Den Broeck, C
van der Sluys, MV
van Veggel, AA
Vass, S
Vaulin, R
Vecchio, A
Veitch, J
Veitch, PJ
Veltkamp, C
Villar, AE
Vorvick, C
Vyachanin, SP
Waldman, SJ
Wallace, L
Wanner, A
Ward, RL
Wei, P
Weinert, M
Weinstein, AJ
Weiss, R
Wen, L
Wen, S
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
White, D
Whiting, BF
Wilkinson, C
Willems, PA
Williams, HR
Williams, L
Willke, B
Winkelmann, L
Winkler, W
Wipf, CC
Wiseman, AG
Woan, G
Wooley, R
Worden, J
Yablon, J
Yakushin, I
Yamamoto, K
Yamamoto, H
Yang, H
Yeaton-Massey, D
Yoshida, S
Yu, P
Zanolin, M
Zhang, L
Zhang, Z
Zhao, C
Zotov, N
Zucker, ME
Zweizig, J
Bizouard, MA
Dietz, A
Guidi, GM
Was, M
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Cumming, A.
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Dahl, K.
Danilishin, S. L.
Dannenberg, R.
Danzmann, K.
Das, K.
Daudert, B.
Daveloza, H.
Davies, G.
Daw, E. J.
Dayanga, T.
Debra, D.
Degallaix, J.
Dent, T.
Dergachev, V.
DeRosa, R.
DeSalvo, R.
Dhurandhar, S.
Di Palma, I.
Diaz, M.
Donovan, F.
Dooley, K. L.
Dorsher, S.
Douglas, E. S. D.
Drever, R. W. P.
Driggers, J. C.
Dumas, J. -C.
Dwyer, S.
Eberle, T.
Edgar, M.
Edwards, M.
Effler, A.
Ehrens, P.
Engel, R.
Etzel, T.
Evans, M.
Evans, T.
Factourovich, M.
Fairhurst, S.
Fan, Y.
Farr, B. F.
Fazi, D.
Fehrmann, H.
Feldbaum, D.
Finn, L. S.
Flanigan, M.
Foley, S.
Forsi, E.
Fotopoulos, N.
Frede, M.
Frei, M.
Frei, Z.
Freise, A.
Frey, R.
Fricke, T. T.
Friedrich, D.
Fritschel, P.
Frolov, V. V.
Fulda, P.
Fyffe, M.
Garcia, J.
Garofoli, J. A.
Gholami, I.
Ghosh, S.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Gill, C.
Goetz, E.
Goggin, L. M.
Gonzalez, G.
Gorodetsky, M. L.
Gossler, S.
Graef, C.
Grant, A.
Gras, S.
Gray, C.
Greenhalgh, R. J. S.
Gretarsson, A. M.
Grosso, R.
Grote, H.
Grunewald, S.
Guido, C.
Gupta, R.
Gustafson, E. K.
Gustafson, R.
Hage, B.
Hallam, J. M.
Hammer, D.
Hammond, G.
Hanks, J.
Hanna, C.
Hanson, J.
Harms, J.
Harry, G. M.
Harry, I. W.
Harstad, E. D.
Hartman, M. T.
Haughian, K.
Hayama, K.
Heefner, J.
Hendry, M. A.
Heng, I. S.
Heptonstall, A. W.
Herrera, V.
Hewitson, M.
Hild, S.
Hoak, D.
Hodge, K. A.
Holt, K.
Hong, T.
Hooper, S.
Hosken, D. J.
Hough, J.
Howell, E. J.
Hughey, B.
Husa, S.
Huttner, S. H.
Ingram, D. R.
Inta, R.
Isogai, T.
Ivanov, A.
Johnson, W. W.
Jones, D. I.
Jones, G.
Jones, R.
Ju, L.
Kalmus, P.
Kalogera, V.
Kandhasamy, S.
Kanner, J. B.
Katsavounidis, E.
Katzman, W.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kells, W.
Kelner, M.
Keppel, D. G.
Khalaidovski, A.
Khalili, F. Y.
Khazanov, E. A.
Kim, N.
Kim, H.
King, P. J.
Kinzel, D. L.
Kissel, J. S.
Klimenko, S.
Kondrashov, V.
Kopparapu, R.
Koranda, S.
Korth, W. Z.
Kozak, D.
Kringel, V.
Krishnamurthy, S.
Krishnan, B.
Kuehn, G.
Kumar, R.
Kwee, P.
Landry, M.
Lantz, B.
Lastzka, N.
Lazzarini, A.
Leaci, P.
Leong, J.
Leonor, I.
Li, J.
Lindquist, P. E.
Lockerbie, N. A.
Lodhia, D.
Lormand, M.
Lu, P.
Luan, J.
Lubinski, M.
Lueck, H.
Lundgren, A. P.
Macdonald, E.
Machenschalk, B.
MacInnis, M.
Mageswaran, M.
Mailand, K.
Mandel, I.
Mandic, V.
Marandi, A.
Marka, S.
Marka, Z.
Maros, E.
Martin, I. W.
Martin, R. M.
Marx, J. N.
Mason, K.
Matichard, F.
Matone, L.
Matzner, R. A.
Mavalvala, N.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
McIntyre, G.
McIver, J.
McKechan, D. J. A.
Meadors, G.
Mehmet, M.
Meier, T.
Melatos, A.
Melissinos, A. C.
Mendell, G.
Mercer, R. A.
Meshkov, S.
Messenger, C.
Meyer, M. S.
Miao, H.
Miller, J.
Mino, Y.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Miyakawa, O.
Moe, B.
Moesta, P.
Mohanty, S. D.
Moraru, D.
Moreno, G.
Mossavi, K.
Mow-Lowry, C. M.
Mueller, G.
Mukherjee, S.
Mullavey, A.
Mueller-Ebhardt, H.
Munch, J.
Murphy, D.
Murray, P. G.
Nash, T.
Nawrodt, R.
Nelson, J.
Newton, G.
Nishizawa, A.
Nolting, D.
Nuttall, L.
O'Reilly, B.
O'Shaughnessy, R.
Ochsner, E.
O'Dell, J.
Ogin, G. H.
Oldenburg, R. G.
Osthelder, C.
Ott, C. D.
Ottaway, D. J.
Ottens, R. S.
Overmier, H.
Owen, B. J.
Page, A.
Pan, Y.
Pankow, C.
Papa, M. A.
Patel, P.
Pedraza, M.
Pekowsky, L.
Penn, S.
Peralta, C.
Perreca, A.
Phelps, M.
Pickenpack, M.
Pinto, I. M.
Pitkin, M.
Pletsch, H. J.
Plissi, M. V.
Podkaminer, J.
Poeld, J.
Postiglione, F.
Predoi, V.
Price, L. R.
Prijatelj, M.
Principe, M.
Privitera, S.
Prix, R.
Prokhorov, L.
Puncken, O.
Quetschke, V.
Raab, F. J.
Radkins, H.
Raffai, P.
Rakhmanov, M.
Ramet, C. R.
Rankins, B.
Mohapatra, S. R. P.
Raymond, V.
Redwine, K.
Reed, C. M.
Reed, T.
Reid, S.
Reitze, D. H.
Riesen, R.
Riles, K.
Roberts, P.
Robertson, N. A.
Robinson, C.
Robinson, E. L.
Roddy, S.
Rollins, J.
Romano, J. D.
Romie, J. H.
Roever, C.
Rowan, S.
Ruediger, A.
Ryan, K.
Sakata, S.
Sakosky, M.
Salemi, F.
Salit, M.
Sammut, L.
Sancho de la Jordana, L.
Sandberg, V.
Sannibale, V.
Santamaria, L.
Santiago-Prieto, I.
Santostasi, G.
Saraf, S.
Sathyaprakash, B. S.
Sato, S.
Saulson, P. R.
Savage, R.
Schilling, R.
Schlamminger, S.
Schnabel, R.
Schofield, R. M. S.
Schulz, B.
Schutz, B. F.
Schwinberg, P.
Scott, J.
Scott, S. M.
Searle, A. C.
Seifert, F.
Sellers, D.
Sengupta, A. S.
Sergeev, A.
Shaddock, D. A.
Shaltev, M.
Shapiro, B.
Shawhan, P.
Weerathunga, T. Shihan
Shoemaker, D. H.
Sibley, A.
Siemens, X.
Sigg, D.
Singer, A.
Singer, L.
Sintes, A. M.
Skelton, G.
Slagmolen, B. J. J.
Slutsky, J.
Smith, R.
Smith, J. R.
Smith, M. R.
Smith, N. D.
Somiya, K.
Sorazu, B.
Soto, J.
Speirits, F. C.
Stein, A. J.
Steinlechner, J.
Steinlechner, S.
Steplewski, S.
Stefszky, M.
Stochino, A.
Stone, R.
Strain, K. A.
Strigin, S.
Stroeer, A. S.
Stuver, A. L.
Summerscales, T. Z.
Sung, M.
Susmithan, S.
Sutton, P. J.
Szokoly, G. P.
Talukder, D.
Tanner, D. B.
Tarabrin, S. P.
Taylor, J. R.
Taylor, R.
Thomas, P.
Thorne, K. A.
Thorne, K. S.
Thrane, E.
Thuering, A.
Tokmakov, K. V.
Torres, C.
Torrie, C. I.
Traylor, G.
Trias, M.
Tseng, K.
Ugolini, D.
Urbanek, K.
Vahlbruch, H.
Vaishnav, B.
Vallisneri, M.
Van Den Broeck, C.
van der Sluys, M. V.
van Veggel, A. A.
Vass, S.
Vaulin, R.
Vecchio, A.
Veitch, J.
Veitch, P. J.
Veltkamp, C.
Villar, A. E.
Vorvick, C.
Vyachanin, S. P.
Waldman, S. J.
Wallace, L.
Wanner, A.
Ward, R. L.
Wei, P.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Wen, L.
Wen, S.
Wessels, P.
West, M.
Westphal, T.
Wette, K.
Whelan, J. T.
Whitcomb, S. E.
White, D.
Whiting, B. F.
Wilkinson, C.
Willems, P. A.
Williams, H. R.
Williams, L.
Willke, B.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Woan, G.
Wooley, R.
Worden, J.
Yablon, J.
Yakushin, I.
Yamamoto, K.
Yamamoto, H.
Yang, H.
Yeaton-Massey, D.
Yoshida, S.
Yu, P.
Zanolin, M.
Zhang, L.
Zhang, Z.
Zhao, C.
Zotov, N.
Zucker, M. E.
Zweizig, J.
Bizouard, M. A.
Dietz, A.
Guidi, G. M.
Was, M.
CA LIGO Collaboration
TI IMPLICATIONS FOR THE ORIGIN OF GRB 051103 FROM LIGO OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 051103); gravitational waves; stars:
magnetars
ID GAMMA-RAY BURSTS; GRAVITATIONAL-WAVE BURSTS; SHORT-DURATION; GIANT
FLARES; SCIENCE RUN; JET BREAKS; SEARCH; REPEATER; GRB-051103;
ENERGETICS
AB We present the results of a LIGO search for gravitational waves (GWs) associated with GRB 051103, a short-duration hard-spectrum gamma-ray burst (GRB) whose electromagnetically determined sky position is coincident with the spiral galaxy M81, which is 3.6 Mpc from Earth. Possible progenitors for short-hard GRBs include compact object mergers and soft gamma repeater (SGR) giant flares. A merger progenitor would produce a characteristic GW signal that should be detectable at a distance of M81, while GW emission from an SGR is not expected to be detectable at that distance. We found no evidence of a GW signal associated with GRB 051103. Assuming weakly beamed gamma-ray emission with a jet semi-angle of 30 degrees, we exclude a binary neutron star merger in M81 as the progenitor with a confidence of 98%. Neutron star-black hole mergers are excluded with >99% confidence. If the event occurred in M81, then our findings support the hypothesis that GRB 051103 was due to an SGR giant flare, making it one of the most distant extragalactic magnetars observed to date.
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RP Abadie, J (reprint author), LIGO Calif Inst Technol, Pasadena, CA 91125 USA.
RI Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014; Finn, Lee
Samuel/A-3452-2009; Sigg, Daniel/I-4308-2015; Graef,
Christian/J-3167-2015; Ottaway, David/J-5908-2015; Shaddock,
Daniel/A-7534-2011; Postiglione, Fabio/O-4744-2015; Gehring,
Tobias/A-8596-2016; Howell, Eric/H-5072-2014; Ott,
Christian/G-2651-2011; Pinto, Innocenzo/L-3520-2016; Harms,
Jan/J-4359-2012; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016;
Hild, Stefan/A-3864-2010; Martin, Iain/A-2445-2010; Pitkin,
Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Miao,
Haixing/O-1300-2013; Khazanov, Efim/B-6643-2014; Salemi,
Francesco/F-6988-2014; Nelson, John/H-7215-2014; Danilishin,
Stefan/K-7262-2012; Khalili, Farit/D-8113-2012; McClelland,
David/E-6765-2010; Vecchio, Alberto/F-8310-2015; Mow-Lowry,
Conor/F-8843-2015; Ju, Li/C-2623-2013; Steinlechner,
Sebastian/D-5781-2013; Costa, Cesar/G-7588-2012; Bell,
Angus/E-7312-2011; Prokhorov, Leonid/I-2953-2012; Gorodetsky,
Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov,
Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012;
Chen, Yanbei/A-2604-2013; Strain, Kenneth/D-5236-2011; Zhao,
Chunnong/C-2403-2013
OI Principe, Maria/0000-0002-6327-0628; Douglas, Ewan/0000-0002-0813-4308;
Kanner, Jonah/0000-0001-8115-0577; O'Shaughnessy,
Richard/0000-0001-5832-8517; Freise, Andreas/0000-0001-6586-9901;
Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard
F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Veitch,
John/0000-0002-6508-0713; Farr, Ben/0000-0002-2916-9200; Guidi,
Gianluca/0000-0002-3061-9870; Santamaria, Lucia/0000-0002-5986-0449;
Hallam, Jonathan Mark/0000-0002-7087-0461; Nishizawa,
Atsushi/0000-0003-3562-0990; Scott, Jamie/0000-0001-6701-6515; Sorazu,
Borja/0000-0002-6178-3198; Zweizig, John/0000-0002-1521-3397; Ward,
Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Fairhurst,
Stephen/0000-0001-8480-1961; Matichard, Fabrice/0000-0001-8982-8418;
Husa, Sascha/0000-0002-0445-1971; Papa,
M.Alessandra/0000-0002-1007-5298; Aulbert, Carsten/0000-0002-1481-8319;
Pinto, Innocenzo M./0000-0002-2679-4457; Finn, Lee
Samuel/0000-0002-3937-0688; Sigg, Daniel/0000-0003-4606-6526; Graef,
Christian/0000-0002-4535-2603; Shaddock, Daniel/0000-0002-6885-3494;
Postiglione, Fabio/0000-0003-0628-3796; Gehring,
Tobias/0000-0002-4311-2593; Howell, Eric/0000-0001-7891-2817; Ott,
Christian/0000-0003-4993-2055; Frey, Raymond/0000-0003-0341-2636;
Pitkin, Matthew/0000-0003-4548-526X; Miao, Haixing/0000-0003-4101-9958;
Nelson, John/0000-0002-6928-617X; Danilishin,
Stefan/0000-0001-7758-7493; McClelland, David/0000-0001-6210-5842;
Vecchio, Alberto/0000-0002-6254-1617; Steinlechner,
Sebastian/0000-0003-4710-8548; Bell, Angus/0000-0003-1523-0821;
Gorodetsky, Michael/0000-0002-5159-2742; Allen,
Bruce/0000-0003-4285-6256; Strain, Kenneth/0000-0002-2066-5355; Zhao,
Chunnong/0000-0001-5825-2401
FU Australian Research Council; International Science Linkages program of
the Commonwealth of Australia; Council of Scientific and Industrial
Research of India; Istituto Nazionale di Fisica Nucleare of Italy;
French Centre National de la Recherche Scientifique; Spanish Ministerio
de Educacion y Ciencia; Conselleria d'Economia, Hisenda i Innovacio of
the Govern de les Illes Balears; Royal Society; Scottish Funding
Council; Scottish Universities Physics Alliance; National Aeronautics
and Space Administration; Research Corporation; Alfred P. Sloan
Foundation
FX The authors thank A. Rowlinson and N. Tanvir for bringing GRB 051103 to
our attention. The authors gratefully acknowledge the support of the
United States National Science Foundation for the construction and
operation of the LIGO Laboratory and the Science and Technology
Facilities Council of the United Kingdom, the Max-Planck-Society, and
the State of Niedersachsen/Germany for support of the construction and
operation of the GEO600 detector. The authors also gratefully
acknowledge the support of the research by these agencies and by the
Australian Research Council, the International Science Linkages program
of the Commonwealth of Australia, the Council of Scientific and
Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
of Italy, the French Centre National de la Recherche Scientifique, the
Spanish Ministerio de Educacion y Ciencia, the Conselleria d'Economia,
Hisenda i Innovacio of the Govern de les Illes Balears, the Royal
Society, the Scottish Funding Council, the Scottish Universities Physics
Alliance, The National Aeronautics and Space Administration, the
Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard
Foundation, the Research Corporation, and the Alfred P. Sloan
Foundation. This document has been assigned LIGO Laboratory document
number LIGO-P10000097-v12.
NR 52
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U1 2
U2 30
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2012
VL 755
IS 1
AR 2
DI 10.1088/0004-637X/755/1/2
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500002
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bottacini, E
Brandt, TJ
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Busetto, G
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 Angelis, A
de Palma, F
Dermer, CD
Digel, SW
Silva, ECE
Drell, PS
Drlica-Wagner, A
Falletti, L
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fukazawa, Y
Fukui, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grondin, MH
Grove, JE
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashi, K
Horan, D
Hou, X
Hughes, RE
Itoh, R
Jackson, MS
Johannesson, G
Johnson, AS
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Lee, SH
Lemoine-Goumard, M
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Martin, P
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nemmen, R
Nishino, S
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Romoli, C
Roth, M
Sada, T
Sadrozinski, HFW
Sanchez, DA
Sbarra, C
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Strong, AW
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tibolla, O
Tinivella, M
Torres, DF
Tosti, G
Tramacere, A
Troja, E
Uchiyama, Y
Uehara, T
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Wang, P
Winer, BL
Wood, KS
Yamamoto, H
Yang, Z
Zimmer, S
AF Ackermann, M.
Ajello, M.
Allafort, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Busetto, G.
Buson, S.
Caliandro, G. A.
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 Angelis, A.
de Palma, F.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Falletti, L.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fukazawa, Y.
Fukui, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grondin, M. -H.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashi, K.
Horan, D.
Hou, X.
Hughes, R. E.
Itoh, R.
Jackson, M. S.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Lee, S. -H.
Lemoine-Goumard, M.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Martin, P.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
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.
Nemmen, R.
Nishino, S.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Romoli, C.
Roth, M.
Sada, T.
Sadrozinski, H. F. -W.
Sanchez, D. A.
Sbarra, C.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strong, A. W.
Suson, D. J.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tibolla, O.
Tinivella, M.
Torres, D. F.
Tosti, G.
Tramacere, A.
Troja, E.
Uchiyama, Y.
Uehara, T.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Yamamoto, H.
Yang, Z.
Zimmer, S.
TI FERMI LARGE AREA TELESCOPE STUDY OF COSMIC RAYS AND THE INTERSTELLAR
MEDIUM IN NEARBY MOLECULAR CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; gamma rays: ISM
ID GAMMA-RAYS; CO SURVEY; GALACTIC QUADRANT; MILKY-WAY; EMISSION; GAS;
EGRET; GALAXY; ORION
AB We report an analysis of the interstellar gamma-ray emission from the Chamaeleon, R Coronae Australis (R CrA), and Cepheus and Polaris flare regions with the Fermi Large Area Telescope. They are among the nearest molecular cloud complexes, within similar to 300 pc from the solar system. The gamma-ray emission produced by interactions of cosmic rays (CRs) and interstellar gas in those molecular clouds is useful to study the CR densities and distributions of molecular gas close to the solar system. The obtained gamma-ray emissivities above 250 MeV are (5.9 +/- 0.1(stat-1.0sys)(+0.9)) x 10(-27) photons s(-1) sr(-1) H-atom(-1), (10.2 +/- 0.4(stat-1.7sys)(+1.2)) x 10(-27) photons s(-1) sr(-1) H-atom(-1), and (9.1 +/- 0.3(stat-0.6sys)(+1.5)) x 10(-27) photons s(-1) sr(-1) H-atom(-1) for the Chamaeleon, R CrA, and Cepheus and Polaris flare regions, respectively. Whereas the energy dependences of the emissivities agree well with that predicted from direct CR observations at the Earth, the measured emissivities from 250 MeV to 10 GeV indicate a variation of the CR density by similar to 20% in the neighborhood of the solar system, even if we consider systematic uncertainties. The molecular mass calibrating ratio, X-CO = N(H-2)/W-CO, is found to be (0.96 +/- 0.06(stat-0.12sys)(+0.15)) x 10(20) H-2-molecule cm(-2) (K km s(-1))(-1), (0.99 +/- 0.08(stat-0.10sys)(+0.18)) x 10(20) H-2-molecule cm(-2) (K km s(-1))(-1), and (0.63 +/- 0.02(stat-0.07sys)(+0.09)) x 10(20) H-2-molecule cm(-2) (K km s(-1))(-1) for the Chamaeleon, R CrA, and Cepheus and Polaris flare regions, respectively, suggesting a variation of X-CO in the vicinity of the solar system. From the obtained values of X-CO, the masses of molecular gas traced by W-CO in the Chamaeleon, R CrA, and Cepheus and Polaris flare regions are estimated to be similar to 5 x 10(3)M(circle dot), similar to 10(3)M(circle dot), and similar to 3.3 x 10(4)M(circle dot), respectively. A comparable amount of gas not traced well by standard Hi and CO surveys is found in the regions investigated.
C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.
[Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Busetto, G.; Buson, S.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Busetto, G.; Buson, S.; Pivato, G.; Rando, R.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, 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.
[Brandt, T. J.; Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Brandt, T. J.; Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Chekhtman, A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Parent, D.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
[Ciprini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cohen-Tanugi, J.; Falletti, L.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS IN2P3, Montpellier, France.
[Conrad, J.; Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10693 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, SE-10693 Stockholm, Sweden.
[D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy.
[D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis, I-00133 Rome, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy.
[Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Ferrara, E. C.; Harding, A. K.; McEnery, J. E.; Nemmen, R.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Itoh, R.; Mizuno, T.; Nishino, S.; Sada, T.; Uehara, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Fukui, Y.; Yamamoto, H.] Nagoya Univ, Dept Phys & Astrophys, Nagoya, Aichi 4648602, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Grenier, I. A.] Inst Univ France, F-75005 Paris, France.
[Grondin, M. -H.; Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Grondin, M. -H.] Univ Heidelberg, D-69117 Heidelberg, Germany.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hou, X.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, IN2P3 CNRS, F-33175 Gradignan, France.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Lemoine-Goumard, M.] Univ Bordeaux 1, CNRS IN2p3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Martin, P.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[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.
[Ohno, M.; Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[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.; Sadrozinski, H. F. -W.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Razzano, M.; Sadrozinski, H. F. -W.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 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.
[Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM hayashi@hep01.hepl.hiroshima-u.ac.jp;
mizuno@hep01.hepl.hiroshima-u.ac.jp
RI Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Loparco, Francesco/O-8847-2015; Gargano,
Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Harding,
Alice/D-3160-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013;
Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Nemmen,
Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson,
Gudlaugur/O-8741-2015; 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; Loparco, Francesco/0000-0002-1173-5673;
Gargano, Fabio/0000-0002-5055-6395; Moskalenko,
Igor/0000-0001-6141-458X; Reimer, Olaf/0000-0001-6953-1385; Funk,
Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; De Angelis, Alessandro/0000-0002-3288-2517;
Caraveo, Patrizia/0000-0003-2478-8018; Sgro',
Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X;
Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577;
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; Tramacere,
Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726
FU European Community [ERC-StG-259391]; National Aeronautics and Space
Administration; Department of Energy in the United States; Commissariat
a l'Energie Atomique; Centre National de la Recherche
Scientifique/Institut National de Physique Nucleaire et de Physique des
Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di
Fisica Nucleare in Italy; Ministry of Education, Culture, Sports,
Science, and Technology (MEXT); High Energy Accelerator Research
Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan;
K. A. Wallenberg Foundation; Swedish Research Council; Swedish National
Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy;
Centre National d'Etudes Spatiales in France; NASA [NNX09AC15G]; Max
Planck Society
FX Funded by contract ERC-StG-259391 from the European Community.; The
Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science, and Technology (MEXT), High Energy
Accelerator Research Organization (KEK), and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council, and the Swedish National Space Board in Sweden.;
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. We thank the
GALPROP team for providing a development version of GALPROP model
adjusted to the measurement data by the LAT. GALPROP development is
supported by NASA grant NNX09AC15G and by the Max Planck Society.
NR 33
TC 21
Z9 21
U1 0
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 AUG 10
PY 2012
VL 755
IS 1
AR 22
DI 10.1088/0004-637X/755/1/22
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500022
ER
PT J
AU Geers, VC
Gorti, U
Meyer, MR
Mamajek, E
Benz, AO
Hollenbach, D
AF Geers, Vincent C.
Gorti, Uma
Meyer, Michael R.
Mamajek, Eric
Benz, Arnold O.
Hollenbach, David
TI REMNANT GAS IN EVOLVED CIRCUMSTELLAR DISKS: HERSCHEL PACS OBSERVATIONS
of 10-100 Myr OLD DISK SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planets and satellites: formation; protoplanetary
disks; stars: pre-main sequence
ID SUN-LIKE STARS; X-RAY-RADIATION; LOW-MASS STARS; HR 8799; DEBRIS DISKS;
YOUNG STARS; EXTREME-ULTRAVIOLET; EVOLUTIONARY MODELS; PROTOPLANETARY
DISC; PLANETARY SYSTEMS
AB We present Herschel PACS spectroscopy of the [O I] 63 mu m gas line for three circumstellar disk systems showing signs of significant disk evolution and/or planet formation: HR 8799, HD 377, and RX J1852.3-3700. [O I] is undetected toward HR 8799 and HD 377 with 3 sigma upper limits of 6.8 x 10(-18) W m(-2) and 9.9 x 10(-18) W m(-2), respectively. We find an [O I] detection for RX J1852.3-3700 at (12.3 +/- 1.8) x 10(-18) W m(-2). We use thermochemical disk models to model the gas emission, using constraints on the [O i] 63 mu m and ancillary data to derive gas mass upper limits and constrain gas-to-dust ratios. For HD 377 and HR 8799, we find 3s upper limits on the gas mass of 0.1-20 M-circle plus. For RX J1852.3-3700, we find two distinct disk scenarios that could explain the detection of [O I] 63 mu m and CO(2-1) upper limits reported in the literature: (1) a large disk with gas co-located with the dust (16-500 AU), resulting in a large tenuous disk with similar to 16 M-circle plus of gas, or (2) an optically thick gas disk, truncated at similar to 70 AU, with a gas mass of 150 M-circle plus. We discuss the implications of these results for the formation and evolution of planets in these three systems.
C1 [Geers, Vincent C.; Meyer, Michael R.; Benz, Arnold O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Gorti, Uma] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gorti, Uma; Hollenbach, David] SETI Inst, Mountain View, CA 94043 USA.
[Mamajek, Eric] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
RP Geers, VC (reprint author), ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
EM vcgeers@phys.ethz.ch
FU NASA Herschel Data Analysis program; NASA Astrophysics Data Analysis
Program [NNX09AC78G]; JPL [1433135]; Swiss PRODEX [13911/99/NL/SFe]
FX U.G. and D. H. acknowledge support from grants under the NASA Herschel
Data Analysis program and the NASA Astrophysics Data Analysis Program
(NNX09AC78G) which enabled this work. E. M. acknowledges support from
JPL contract 1433135. This work is based on observations made with
Herschel, a European Space Agency Cornerstone Mission with significant
participation by NASA. Some of the observations were acquired in time
guaranteed by a HIFI hardware contribution funded by Swiss PRODEX (grant
13911/99/NL/SFe). HIFI has been designed and built by a consortium of
institutes and university departments from across Europe, Canada, and
the United States under the leadership of SRON Netherlands Institute for
Space Research, Groningen, The Netherlands, and with major contributions
from Germany, France, and the US. Consortium members are: Canada: CSA,
U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS;
Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico
di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain:
Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia
(CSIC-INTA). Sweden: Chalmers University of Technology-MC2, RSS & GARD;
Onsala Space Observatory; Swedish National Space Board, Stockholm
University-Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA:
Caltech, JPL, NHSC. HIPE is a joint development by the Herschel Science
Ground Segment Consortium, consisting of ESA, the NASA Herschel Science
Center, and the HIFI, PACS, and SPIRE consortia.
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JI Astrophys. J.
PD AUG 10
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500008
ER
PT J
AU Hailey-Dunsheath, S
Sturm, E
Fischer, J
Sternberg, A
Gracia-Carpio, J
Davies, R
Gonzalez-Alfonso, E
Mark, D
Poglitsch, A
Contursi, A
Genzel, R
Lutz, D
Tacconi, L
Veilleux, S
Verma, A
de Jong, JA
AF Hailey-Dunsheath, S.
Sturm, E.
Fischer, J.
Sternberg, A.
Gracia-Carpio, J.
Davies, R.
Gonzalez-Alfonso, E.
Mark, D.
Poglitsch, A.
Contursi, A.
Genzel, R.
Lutz, D.
Tacconi, L.
Veilleux, S.
Verma, A.
de Jong, J. A.
TI HERSCHEL-PACS OBSERVATIONS OF FAR-IR CO LINE EMISSION IN NGC 1068:
HIGHLY EXCITED MOLECULAR GAS IN THE CIRCUMNUCLEAR DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 1068); galaxies: ISM;
galaxies: nuclei; galaxies: Seyfert; infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY NGC-1068; WATER MASER EMISSION;
INFRARED-EMISSION; STAR-FORMATION; SHOCK-WAVES; ISO-SWS; OBSCURING
TORUS; RADIO STRUCTURE; CENTRAL ENGINE
AB We report the detection of far-IR CO rotational emission from the prototypical Seyfert 2 galaxy NGC 1068. Using Herschel-PACS, we have detected 11 transitions in the J(upper) = 14-30 (E-upper/k(B) = 580-2565 K) range, all of which are consistent with arising from within the central 10 '' (700 pc). The detected transitions are modeled as arising from two different components: a moderate-excitation (ME) component close to the galaxy systemic velocity and a high-excitation (HE) component that is blueshifted by similar to 80 km s(-1). We employ a large velocity gradient model and derive n(H2) similar to 10(5.6) cm(-3), T-kin similar to 170 K, and M-H2 similar to 10(6.7) M-circle dot for the ME component and n(H2) similar to 10(6.4) cm(-3), T-kin similar to 570 K, and M-H2 similar to 10(5.6) M-circle dot for the HE component, although for both components the uncertainties in the density and mass are +/-(0.6-0.9) dex. Both components arise from denser and possibly warmer gas than traced by low-J CO transitions, and the ME component likely makes a significant contribution to the mass budget in the nuclear region. We compare the CO line profiles with those of other molecular tracers observed at higher spatial and spectral resolution and find that the ME transitions are consistent with these lines arising in the similar to 200 pc diameter ring of material traced by H-2 1-0 S(1) observations. The blueshift of the HE lines may also be consistent with the bluest regions of this H-2 ring, but a better kinematic match is found with a clump of infalling gas similar to 40 pc north of the active galactic nucleus (AGN). We consider potential heating mechanisms and conclude that X-ray-or shock heating of both components is viable, while far-UV heating is unlikely. We discuss the prospects of placing the HE component near the AGN and conclude that while the moderate thermal pressure precludes an association with the similar to 1 pc radius H2O maser disk, the HE component could potentially be located only a few parsecs more distant from the AGN and might then provide the N-H similar to 10(25) cm(-2) column obscuring the nuclear hard X-rays. Finally, we also report sensitive upper limits extending up to J(upper) = 50, which place constraints on a previous model prediction for the CO emission from the X-ray obscuring torus.
C1 [Hailey-Dunsheath, S.; Sturm, E.; Gracia-Carpio, J.; Davies, R.; Poglitsch, A.; Contursi, A.; Genzel, R.; Lutz, D.; Tacconi, L.; de Jong, J. A.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Fischer, J.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Sternberg, A.; Mark, D.] Tel Aviv Univ, Sackler Sch Phys & Astron, IL-69978 Ramat Aviv, Israel.
[Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain.
[Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, S.] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Verma, A.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
RP Hailey-Dunsheath, S (reprint author), CALTECH, Mail Code 301-17,1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM shd@astro.caltech.edu
FU US ONR; NHSC; DFG [STE1869/1-1.GE625/15-1]; Spanish Ministerio de
Ciencia e Innovacion [AYA2010-21697-C05-01]; Senior NPP from NASA;
BMVIT(Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain)
FX We thank Eva Schinnerer for generously providing her IRAM PdBI CO(1-0)
and CO(2-1) data and Francisco Muller Sanchez for providing his
SINFONI/VLT H2 1-0 S(1) map. We also thank an anonymous
referee for many helpful comments on an early draft of this manuscript.
Basic research in IR astronomy at NRL is funded by the US ONR; J.F. also
acknowledges support from the NHSC. We thank the DFG for support via
German-Israel Project Cooperation grant STE1869/1-1.GE625/15-1. E. G.-A.
thanks the support by the Spanish Ministerio de Ciencia e Innovacion
under project AYA2010-21697-C05-01 and is a Research Associate at the
Harvard-Smithsonian Center for Astrophysics. S. V. acknowledges support
from a Senior NPP Award from NASA and thanks the host institution, the
Goddard Space Flight Center. 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).
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JI Astrophys. J.
PD AUG 10
PY 2012
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DI 10.1088/0004-637X/755/1/57
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500057
ER
PT J
AU Helton, LA
Gehrz, RD
Woodward, CE
Wagner, RM
Vacca, WD
Evans, A
Krautter, J
Schwarz, GJ
Shenoy, DP
Starrfield, S
AF Helton, L. Andrew
Gehrz, Robert D.
Woodward, Charles E.
Wagner, R. Mark
Vacca, William D.
Evans, Aneurin
Krautter, Joachim
Schwarz, Greg J.
Shenoy, Dinesh P.
Starrfield, Sumner
TI ELEMENTAL ABUNDANCES IN THE EJECTA OF OLD CLASSICAL NOVAE FROM
LATE-EPOCH SPITZER SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; novae, cataclysmic variables; stars: abundances; stars:
individual (V1974 Cygni, V382 Velorum, V1494 Aquilae)
ID ELECTRON-IMPACT EXCITATION; EFFECTIVE COLLISION STRENGTHS;
FINE-STRUCTURE LEVELS; 1999 NO. 2; V1974 CYGNI; V1494 AQUILAE; TEMPORAL
EVOLUTION; SPACE-TELESCOPE; IRON PROJECT; LIGHT CURVES
AB We present Spitzer Space Telescope mid-infrared IRS spectra, supplemented by ground-based optical observations, of the classical novae V1974 Cyg, V382Vel, and V1494 Aql more than 11, 8, and 4 years after outburst, respectively. The spectra are dominated by forbidden emission from neon and oxygen, though in some cases, there are weak signatures of magnesium, sulfur, and argon. We investigate the geometry and distribution of the late time ejecta by examination of the emission line profiles. Using nebular analysis in the low-density regime, we estimate lower limits on the abundances in these novae. In V1974 Cyg and V382 Vel, our observations confirm the abundance estimates presented by other authors and support the claims that these eruptions occurred on ONe white dwarfs (WDs). We report the first detection of neon emission in V1494 Aql and show that the system most likely contains a COWD.
C1 [Helton, L. Andrew; Vacca, William D.] NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gehrz, Robert D.; Woodward, Charles E.; Shenoy, Dinesh P.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Wagner, R. Mark] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Evans, Aneurin] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Krautter, Joachim] Heidelberg Univ, Landessternwarte Zentrum Astron, D-69117 Heidelberg, Germany.
[Schwarz, Greg J.] Amer Astron Soc, Washington, DC 20009 USA.
[Starrfield, Sumner] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Helton, LA (reprint author), NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, MS N232-11, Moffett Field, CA 94035 USA.
EM ahelton@sofia.usra.edu
OI Schwarz, Gregory/0000-0002-0786-7307
FU NASA/JPL Spitzer [1289430, 1314757, 1267992, 1256406, 1215746]; The
United States Air Force; National Science Foundation; NSF; NASA; Spitzer
FX L.A.H., C. E. W., and R. D. G. were supported in part by NASA/JPL
Spitzer grants 1289430, 1314757, 1267992, 1256406, and 1215746 to the
University of Minnesota, The United States Air Force, as well as various
National Science Foundation grants. S. S. acknowledges partial support
from NSF, NASA, and Spitzer grants to ASU.
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J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2012
VL 755
IS 1
AR 37
DI 10.1088/0004-637X/755/1/37
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500037
ER
PT J
AU Pietrobon, D
Gorski, KM
Bartlett, J
Banday, AJ
Dobler, G
Colombo, LPL
Hildebrandt, SR
Jewell, JB
Pagano, L
Rocha, G
Eriksen, HK
Saha, R
Lawrence, CR
AF Pietrobon, Davide
Gorski, Krzysztof M.
Bartlett, James
Banday, A. J.
Dobler, Gregory
Colombo, Loris P. L.
Hildebrandt, Sergi R.
Jewell, Jeffrey B.
Pagano, Luca
Rocha, Graca
Eriksen, Hans Kristian
Saha, Rajib
Lawrence, Charles R.
TI ANALYSIS OF WMAP 7 YEAR TEMPERATURE DATA: ASTROPHYSICS OF THE GALACTIC
HAZE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic microwave background; cosmology: observations; diffuse radiation;
Galaxy: center; methods: data analysis; methods: numerical; methods:
statistical
ID MICROWAVE-ANISOTROPY-PROBE; BAYESIAN COMPONENT SEPARATION; POWER
SPECTRUM ESTIMATION; SPINNING DUST GRAINS; GAMMA-RAY HAZE; FOREGROUND
EMISSION; BACKGROUND DATA; 5-YEAR DATA; SKY MAPS; RADIATION
AB We perform a joint analysis of the cosmic microwave background (CMB) and Galactic emission from the WMAP 7 year temperature data. Using the Commander code, based on Gibbs sampling, we simultaneously derive the CMB and Galactic components on scales larger than 1. with improved sensitivity over previous work. We conduct a detailed study of the low-frequency Galactic foreground, focusing on the "microwave haze" emission around the Galactic center. We demonstrate improved performance in quantifying the diffuse Galactic emission when including Haslam 408 MHz data and when jointly modeling the spinning and thermal dust emission. We examine whether the hypothetical Galactic haze can be explained by a spatial variation of the synchrotron spectral index, and find that the excess of emission around the Galactic center is stable with respect to variations of the foreground model. Our results demonstrate that the new Galactic foreground component-the microwave haze-is indeed present.
C1 [Pietrobon, Davide; Gorski, Krzysztof M.; Bartlett, James; Colombo, Loris P. L.; Jewell, Jeffrey B.; Pagano, Luca; Rocha, Graca; Lawrence, Charles R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gorski, Krzysztof M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Bartlett, James] Univ Paris Diderot, Lab AstroParticule & Cosmol APC, CEA Lrfu, Observ Paris,CNRS,IN2P3, F-75205 Paris 13, France.
[Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Banday, A. J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Dobler, Gregory] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Colombo, Loris P. L.] Univ So Calif, USC Dana & David Dornsife Coll Letters Arts & Sci, Los Angeles, CA 90089 USA.
[Hildebrandt, Sergi R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Eriksen, Hans Kristian] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Eriksen, Hans Kristian] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway.
[Saha, Rajib] Indian Inst Sci Educ & Res Bhopal, Dept Phys, Bhopal 462023, MP, India.
RP Pietrobon, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM davide.pietrobon@jpl.nasa.gov
RI Colombo, Loris/J-2415-2016
OI Colombo, Loris/0000-0003-4572-7732
FU NASA Office of Space Science; Institut Universitaire de France; Harrey
L. Karp discovery award
FX Many of the results in this paper have been derived using the HEALPix
(Gorski et al. 2005) software and analysis package. We acknowledge use
of the Legacy Archive for Microwave Background Data Analysis (LAMBDA).
Support for LAMBDA is provided by the NASA Office of Space Science.
J.G.B. gratefully acknowledges support by the Institut Universitaire de
France. G. D. has been supported by the Harrey L. Karp discovery award.
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EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2012
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DI 10.1088/0004-637X/755/1/69
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500069
ER
PT J
AU Reichardt, CL
Shaw, L
Zahn, O
Aird, KA
Benson, BA
Bleem, LE
Carlstrom, JE
Chang, CL
Cho, HM
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Dudley, J
George, EM
Halverson, NW
Holder, GP
Holzapfel, WL
Hoover, S
Hou, Z
Hrubes, JD
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
McMahon, JJ
Mehl, J
Meyer, SS
Millea, M
Mohr, JJ
Montroy, TE
Natoli, T
Padin, S
Plagge, T
Pryke, C
Ruhl, JE
Schaffer, KK
Shirokoff, E
Spieler, HG
Staniszewski, Z
Stark, AA
Story, K
van Engelen, A
Vanderlinde, K
Vieira, JD
Williamson, R
AF Reichardt, C. L.
Shaw, L.
Zahn, O.
Aird, K. A.
Benson, B. A.
Bleem, L. E.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Dudley, J.
George, E. M.
Halverson, N. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hou, Z.
Hrubes, J. D.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Millea, M.
Mohr, J. J.
Montroy, T. E.
Natoli, T.
Padin, S.
Plagge, T.
Pryke, C.
Ruhl, J. E.
Schaffer, K. K.
Shirokoff, E.
Spieler, H. G.
Staniszewski, Z.
Stark, A. A.
Story, K.
van Engelen, A.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
TI A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH
TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology:
observations; diffuse radiation; large-scale structure of universe
ID ATACAMA COSMOLOGY TELESCOPE; ZELDOVICH POWER SPECTRUM; STAR-FORMING
GALAXIES; EXTRAGALACTIC SOURCES; CLUSTERS; PARAMETERS; PROBE; SKY;
CONSTRAINTS; CATALOG
AB We present the first three-frequency South Pole Telescope (SPT) cosmic microwave background (CMB) power spectra. The band powers presented here cover angular scales 2000 < l < 9400 in frequency bands centered at 95, 150, and 220 GHz. At these frequencies and angular scales, a combination of the primary CMB anisotropy, thermal and kinetic Sunyaev-Zel'dovich (SZ) effects, radio galaxies, and cosmic infrared background (CIB) contributes to the signal. We combine Planck/HFI and SPT data at 220 GHz to constrain the amplitude and shape of the CIB power spectrum and find strong evidence for nonlinear clustering. We explore the SZ results using a variety of cosmological models for the CMB and CIB anisotropies and find them to be robust with one exception: allowing for spatial correlations between the thermal SZ effect and CIB significantly degrades the SZ constraints. Neglecting this potential correlation, we find the thermal SZ power at 150 GHz and l = 3000 to be 3.65 +/- 0.69 mu K-2, and set an upper limit on the kinetic SZ power to be less than 2.8 mu K-2 at 95% confidence. When a correlation between the thermal SZ and CIB is allowed, we constrain a linear combination of thermal and kinetic SZ power: D-3000(tSZ) + 0.5(3000)(DkSZ) = 4.60 +/- 0.63 mu K-2, consistent with earlier measurements. We use the measured thermal SZ power and an analytic, thermal SZ model calibrated with simulations to determine sigma(8) = 0.807 +/- 0.016. Modeling uncertainties involving the astrophysics of the intracluster medium rather than the statistical uncertainty in the measured band powers are the dominant source of uncertainty on sigma(8). We also place an upper limit on the kinetic SZ power produced by patchy reionization; a companion paper uses these limits to constrain the reionization history of the universe.
C1 [Reichardt, C. L.; Shaw, L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Keisler, R.; Meyer, S. S.; Natoli, T.; Pryke, C.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Joy, M.] NASA, Dept Space Sci, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Reichardt, CL (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
EM cr@bolo.berkeley.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; Stark,
Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics
Frontier Center [PHY-0114422]; National Sciences and Engineering
Research Council of Canada; Canada Research Chairs program; Canadian
Institute for Advanced Research; NASA [HF-51275.01]; KICP; Alfred P.
Sloan Research Fellowship; Yale University; NSF [AST-1009811, 0709498];
Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231];
NASA Office of Space Science; Kavli Foundation; Gordon and Betty Moore
Foundation
FX We thank Cien Shang, Guilaine Lagache, Olivier Dore, and Marco Viero for
useful discussions and assistance with the CIB modeling. The South Pole
Telescope is supported by the National Science Foundation through grants
ANT-0638937 and ANT-0130612. Partial support is also provided by the NSF
Physics Frontier Center grant PHY-0114422 to the Kavli Institute of
Cosmological Physics at the University of Chicago, the Kavli Foundation,
and the Gordon and Betty Moore Foundation. The McGill group acknowledges
funding from the National Sciences and Engineering Research Council of
Canada, Canada Research Chairs program, and the Canadian Institute for
Advanced Research. R. K. acknowledges support from NASA Hubble
Fellowship grant HF-51275.01. B. A. B. is supported by a KICP
Fellowship. M. D. acknowledges support from an Alfred P. Sloan Research
Fellowship. L. S. acknowledges the support of Yale University and NSF
grant AST-1009811. M. M. and L. K. acknowledge the support of NSF grant
0709498. This research used resources of the National Energy Research
Scientific Computing Center, which is supported by the Office of Science
of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.
Some of the results in this paper have been derived using the HEALPix
(Gorski et al. 2005) package. 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2012
VL 755
IS 1
AR 70
DI 10.1088/0004-637X/755/1/70
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500070
ER
PT J
AU Sudol, JJ
Haghighipour, N
AF Sudol, Jeffrey J.
Haghighipour, Nader
TI HIGH-MASS, FOUR-PLANET CONFIGURATIONS FOR HR 8799: CONSTRAINING THE
ORBITAL INCLINATION AND AGE OF THE SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: dynamical evolution and stability; stars:
individual (HR 8799)
ID DUSTY DEBRIS DISKS; PLANETARY SYSTEM; ASTEROSEISMOLOGY; STABILITY;
DORADUS; STARS; IRAS
AB Debates regarding the age and inclination of the planetary system orbiting HR 8799, and the release of additional astrometric data following the discovery of the fourth planet, prompted us to examine the possibility of constraining these two quantities by studying the long-term stability of this system at different orbital inclinations and in its high-mass configuration (7-10-10-10M(Jup)). We carried out similar to 1.5 million N-body integrations for different combinations of orbital elements of the four planets. The most dynamically stable combinations survived less than similar to 5Myr at inclinations of 0 degrees and 13 degrees, and 41, 46, and 31 Myr at 18 degrees, 23 degrees, and 30 degrees, respectively. Given such short lifetimes and the location of the system on the age-luminosity diagram for low-mass objects, the most reasonable conclusion of our study is that the planetary masses are less than 7-10-10-10M(Jup) and the system is quite young. Two trends to note from our work are as follows. (1) In the most stable systems, the higher the inclination, the more the coordinates for planets b and c diverge from the oldest archival astrometric data (released after we completed our N-body integrations), suggesting that either these planets are in eccentric orbits or have lower orbital inclinations than that of planet d. (2) The most stable systems place planet e closer to the central star than is observed, supporting the conclusion that the planets are more massive and the system is young. We present the details of our simulations and discuss the implications of the results.
C1 [Sudol, Jeffrey J.] W Chester Univ, Dept Phys, W Chester, PA 19383 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Sudol, JJ (reprint author), W Chester Univ, Dept Phys, 720 S Church St, W Chester, PA 19383 USA.
EM jsudol@wcupa.edu; nader@ifa.hawaii.edu
FU West Chester University College of Arts and Sciences; West Chester
University Department of Physics; NASA Astrobiology Institute at
Institute for Astronomy, University of Hawaii [NNA09DA77]; NASA EXOB
grant [NNX09AN05G]
FX This project has been partially funded by a Support and Development
Award from the West Chester University College of Arts and Sciences to
J.J.S. and by the West Chester University Department of Physics. N.H.
acknowledges support from the NASA Astrobiology Institute under
Cooperative Agreement NNA09DA77 at the Institute for Astronomy,
University of Hawaii, and NASA EXOB grant NNX09AN05G. We thank J. T.
Singh, Coordinator of Technical Support Services in Academic Computing
at West Chester University, for contributing decommissioned computers to
this project. We also thank the following undergraduate students at West
Chester University who helped us to complete the construction of the
computer network used in this project and to conduct some early
investigations of the HR 8799 system: Steve Assalita, Brittany
Johnstone, Nora Pearse, Michael Savoy, and Michael Scott.
NR 26
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2012
VL 755
IS 1
AR 38
DI 10.1088/0004-637X/755/1/38
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500038
ER
PT J
AU Toala, JA
Guerrero, MA
Chu, YH
Gruendl, RA
Arthur, SJ
Smith, RC
Snowden, SL
AF Toala, J. A.
Guerrero, M. A.
Chu, Y-H
Gruendl, R. A.
Arthur, S. J.
Smith, R. C.
Snowden, S. L.
TI X-RAY EMISSION FROM THE WOLF-RAYET BUBBLE S 308
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: bubbles; ISM: individual objects (S 308); stars: individual (HD
50896); stars: winds, outflows; stars: Wolf-Rayet; X-rays: individual (S
308)
ID BLOWN INTERSTELLAR BUBBLES; SPATIALLY RESOLVED SPECTROSCOPY; WR RING
NEBULAE; TIME SEQUENCE O; MASSIVE STARS; XMM-NEWTON; DYNAMICAL
EVOLUTION; CIRCUMSTELLAR GAS; ENERGY-BALANCE; ABUNDANCES
AB The Wolf-Rayet (WR) bubble S 308 around the WR star HD 50896 is one of the only two WR bubbles known to possess X-ray emission. We present XMM-Newton observations of three fields of this WR bubble that, in conjunction with an existing observation of its northwest quadrant, map most of the nebula. The X-ray emission from S 308 displays a limb-brightened morphology, with a central cavity similar to 22' in size and a shell thickness of similar to 8'. This X-ray shell is confined by the optical shell of ionized material. The spectrum is dominated by the He-like triplets of N VI at 0.43 keV and O VII at 0.57 keV, and declines toward high energies, with a faint tail up to 1 keV. This spectrum can be described by a two-temperature optically thin plasma emission model (T-1 similar to 1.1 x 10(6) K, T-2 similar to 13 x 10(6) K), with a total X-ray luminosity similar to 2 x 10(33) erg s(-1) at the assumed distance of 1.5 kpc.
C1 [Toala, J. A.; Guerrero, M. A.] CSIC, IAA, E-18008 Granada, Spain.
[Toala, J. A.; Arthur, S. J.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico.
[Chu, Y-H; Gruendl, R. A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Smith, R. C.] NOAO CTIO, Tucson, AZ 85719 USA.
[Snowden, S. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Toala, JA (reprint author), CSIC, IAA, Glorieta Astron S-N, E-18008 Granada, Spain.
EM toala@iaa.es
OI Guerrero, Martin/0000-0002-7759-106X
FU NASA XMM-Newton Guest Observer Program [NNG 04GH99G]; DGAPA-UNAM [PAPIIT
IN100309]; CONACyT; CONACyT-SNI (Mexico); CSIC JAE-PREDOC (Spain);
Spanish Ministerio de Economia y Competitividad [AYA2001-29754-C03-02]
FX This research was supported by the NASA XMM-Newton Guest Observer
Program grant NNG 04GH99G. S.J.A. and J.A.T. acknowledge financial
support from DGAPA-UNAM through grant PAPIIT IN100309. J.A.T. also
thanks CONACyT, CONACyT-SNI (Mexico), and CSIC JAE-PREDOC (Spain) for a
student grant. J.A.T. and M. A. G. are partially funded by grant
AYA2001-29754-C03-02 of the Spanish Ministerio de Economia y
Competitividad.
NR 48
TC 15
Z9 15
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2012
VL 755
IS 1
AR 77
DI 10.1088/0004-637X/755/1/77
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500077
ER
PT J
AU Umetsu, K
Medezinski, E
Nonino, M
Merten, J
Zitrin, A
Molino, A
Grillo, C
Carrasco, M
Donahue, M
Mahdavi, A
Coe, D
Postman, M
Koekemoer, A
Czakon, N
Sayers, J
Mroczkowski, T
Golwala, S
Koch, PM
Lin, KY
Molnar, SM
Rosati, P
Balestra, I
Mercurio, A
Scodeggio, M
Biviano, A
Anguita, T
Infante, L
Seidel, G
Sendra, I
Jouvel, S
Host, O
Lemze, D
Broadhurst, T
Meneghetti, M
Moustakas, L
Bartelmann, M
Benitez, N
Bouwens, R
Bradley, L
Ford, H
Jimenez-Teja, Y
Kelson, D
Lahav, O
Melchior, P
Moustakas, J
Ogaz, S
Seitz, S
Zheng, W
AF Umetsu, Keiichi
Medezinski, Elinor
Nonino, Mario
Merten, Julian
Zitrin, Adi
Molino, Alberto
Grillo, Claudio
Carrasco, Mauricio
Donahue, Megan
Mahdavi, Andisheh
Coe, Dan
Postman, Marc
Koekemoer, Anton
Czakon, Nicole
Sayers, Jack
Mroczkowski, Tony
Golwala, Sunil
Koch, Patrick M.
Lin, Kai-Yang
Molnar, Sandor M.
Rosati, Piero
Balestra, Italo
Mercurio, Amata
Scodeggio, Marco
Biviano, Andrea
Anguita, Timo
Infante, Leopoldo
Seidel, Gregor
Sendra, Irene
Jouvel, Stephanie
Host, Ole
Lemze, Doron
Broadhurst, Tom
Meneghetti, Massimo
Moustakas, Leonidas
Bartelmann, Matthias
Benitez, Narciso
Bouwens, Rychard
Bradley, Larry
Ford, Holland
Jimenez-Teja, Yolanda
Kelson, Daniel
Lahav, Ofer
Melchior, Peter
Moustakas, John
Ogaz, Sara
Seitz, Stella
Zheng, Wei
TI CLASH: MASS DISTRIBUTION IN AND AROUND MACS J1206.2-0847 FROM A FULL
CLUSTER LENSING ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; dark matter; galaxies: clusters: individual
(MACS J1206.2-0847); gravitational lensing: strong; gravitational
lensing: weak
ID HUBBLE-SPACE-TELESCOPE; DARK-MATTER HALOS; ZELDOVICH EFFECT
OBSERVATIONS; HIGH-REDSHIFT CLUSTERS; LARGE-SCALE STRUCTURE; DEEP
ADVANCED CAMERA; LAMBDA-CDM CLUSTERS; DIGITAL SKY SURVEY;
X-RAY-CLUSTERS; GALAXY CLUSTERS
AB We derive an accurate mass distribution of the galaxy cluster MACS J1206.2-0847 (z = 0.439) from a combined weak-lensing distortion, magnification, and strong-lensing analysis of wide-field Subaru BVR(c)I(c)z' imaging and our recent 16-band Hubble Space Telescope observations taken as part of the Cluster Lensing And Supernova survey with Hubble program. We find good agreement in the regions of overlap between several weak-and strong-lensing mass reconstructions using a wide variety of modeling methods, ensuring consistency. The Subaru data reveal the presence of a surrounding large-scale structure with the major axis running approximately northwest-southeast (NW-SE), aligned with the cluster and its brightest galaxy shapes, showing elongation with a similar to 2:1 axis ratio in the plane of the sky. Our full-lensing mass profile exhibits a shallow profile slope d ln Sigma/d ln R similar to -1 at cluster outskirts (R greater than or similar to 1 Mpc h(-1)), whereas the mass distribution excluding the NW-SE excess regions steepens farther out, well described by the Navarro-Frenk-White form. Assuming a spherical halo, we obtain a virial mass M-vir = (1.1 +/- 0.2 +/- 0.1) x 10(15) M-circle dot h(-1) and a halo concentration c(vir) = 6.9 +/- 1.0 +/- 1.2 (c(vir) similar to 5.7 when the central 50 kpc h(-1) is excluded), which falls in the range 4 less than or similar to < c > less than or similar to 7 of average c(M, z) predictions for relaxed clusters from recent. cold dark matter simulations. Our full-lensing results are found to be in agreement with X-ray mass measurements where the data overlap, and when combined with Chandra gas mass measurements, they yield a cumulative gas mass fraction of 13.7(-3.0)(+4.5)% at 0.7 Mpc h(-1) (approximate to 1.7 r(2500)), a typical value observed for high-mass clusters.
C1 [Umetsu, Keiichi; Koch, Patrick M.; Lin, Kai-Yang] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Medezinski, Elinor; Lemze, Doron; Ford, Holland; Zheng, Wei] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Nonino, Mario; Balestra, Italo; Biviano, Andrea] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Merten, Julian; Mroczkowski, Tony; Moustakas, Leonidas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zitrin, Adi; Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, ZAH, Heidelberg, Germany.
[Molino, Alberto; Benitez, Narciso; Jimenez-Teja, Yolanda] Inst Astrofis Andalucia CSIC, Granada, Spain.
[Grillo, Claudio] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Carrasco, Mauricio; Anguita, Timo; Infante, Leopoldo] Pontificia Univ Catolica Chile, Ctr Astroingn, Dept Astron & Astrofis, Santiago, Chile.
[Carrasco, Mauricio; Rosati, Piero] European So Observ, D-85748 Garching, Germany.
[Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Mahdavi, Andisheh] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA USA.
[Coe, Dan; Postman, Marc; Koekemoer, Anton; Bradley, Larry; Ogaz, Sara] Space Telescope Sci Inst, Baltimore, MD 21208 USA.
[Czakon, Nicole; Sayers, Jack; Mroczkowski, Tony; Golwala, Sunil] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Molnar, Sandor M.] Natl Taiwan Univ, LeCosPA Ctr, Taipei 10617, Taiwan.
[Mercurio, Amata] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Scodeggio, Marco] INAF IASF Milano, I-20133 Milan, Italy.
[Anguita, Timo; Seidel, Gregor] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Sendra, Irene; Broadhurst, Tom] Univ Basque Country, Dept Theoret Phys & Hist Sci, UPV EHU, Bilbao 48080, Spain.
[Jouvel, Stephanie; Host, Ole; Lahav, Ofer] UCL, Dept Phys & Astron, London, England.
[Jouvel, Stephanie] Inst Ciencies Espai IEEC CSIC, E-08193 Bellaterra, Barcelona, Spain.
[Broadhurst, Tom] Ikerbasque, Basque Fdn Sci, Bilbao 48011, Spain.
[Meneghetti, Massimo] Osservatorio Astron Bologna, INAF, Bologna, Italy.
[Meneghetti, Massimo] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
[Bouwens, Rychard] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Kelson, Daniel] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Moustakas, John] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Seitz, Stella] Univ Sternwarte, D-81679 Munich, Germany.
RP Umetsu, K (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
EM keiichi@asiaa.sinica.edu.tw
RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014;
Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015;
Meneghetti, Massimo/O-8139-2015;
OI Biviano, Andrea/0000-0002-0857-0732; Moustakas,
Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048;
Benitez, Narciso/0000-0002-0403-7455; Scodeggio,
Marco/0000-0002-2282-5850; Mroczkowski, Tony/0000-0003-3816-5372;
Grillo, Claudio/0000-0002-5926-7143; Meneghetti,
Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662;
Balestra, Italo/0000-0001-9660-894X; Sendra, Irene/0000-0002-1148-8377;
Umetsu, Keiichi/0000-0002-7196-4822
FU NASA [NAS 5-26555, NAS 5-32864, HST-GO-12065.01-A]; National Science
Council of Taiwan [NSC100-2112-M-001-008-MY3]; PRIN INAF; Academia
Sinica Career Development Award; ESO Paranal Observatory [186.A-0798];
DFG cluster of excellence Origin and Structure of the Universe; NASA
Graduate Student Research Fellowship; "Internationale Spitzenforschung
II/2" of the Baden-Wurttemberg Stiftung; Dark Cosmology Centre; Danish
National Research Foundation; Spanish Ministry of Economy and
Competitiveness [FIS2010-15492]; NASA through the Einstein Fellowship
Program [PF0-110077]; [NSF/AST0838261]; [NASA/NNX11AB07G]
FX The CLASH Multi-Cycle Treasury Program is based on observations made
with the NASA/ESA Hubble Space Telescope. The Space Telescope Science
Institute is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS 5-26555. ACS was developed
under NASA contract NAS 5-32864. This research is supported in part by
NASA grant HST-GO-12065.01-A, National Science Council of Taiwan grant
NSC100-2112-M-001-008-MY3, and PRIN INAF 2010. K. U. acknowledges
support from the Academia Sinica Career Development Award. Part of this
work is based on data collected at the Very Large Telescope at the ESO
Paranal Observatory, under Programme ID 186.A-0798. P. R., C. G., I. B.,
and S. S. acknowledge partial support by the DFG cluster of excellence
Origin and Structure of the Universe. The Bolocam observations were
partially supported by the Gordon and Betty Moore Foundation. J.S. was
supported by NSF/AST0838261 and NASA/NNX11AB07G; N.C. was partially
supported by a NASA Graduate Student Research Fellowship. A.Z. is
supported by the "Internationale Spitzenforschung II/2" of the
Baden-Wurttemberg Stiftung. C. G. acknowledges support from the Dark
Cosmology Centre, which is funded by the Danish National Research
Foundation. I. S. holds a PhD FPI Fellowship contract from the Spanish
Ministry of Economy and Competitiveness and is also supported by the
mentioned ministry through research project FIS2010-15492. Support for
T. M. was provided by NASA through the Einstein Fellowship Program,
grant PF0-110077.
NR 157
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2012
VL 755
IS 1
AR 56
DI 10.1088/0004-637X/755/1/56
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500056
ER
PT J
AU van Eyken, JC
Ciardi, DR
von Braun, K
Kane, SR
Plavchan, P
Bender, CF
Brown, TM
Crepp, JR
Fulton, BJ
Howard, AW
Howell, SB
Mahadevan, S
Marcy, GW
Shporer, A
Szkody, P
Akeson, RL
Beichman, CA
Boden, AF
Gelino, DM
Hoard, DW
Ramirez, SV
Rebull, LM
Stauffer, JR
Bloom, JS
Cenko, SB
Kasliwal, MM
Kulkarni, SR
Law, NM
Nugent, PE
Ofek, EO
Poznanski, D
Quimby, RM
Walters, R
Grillmair, CJ
Laher, R
Levitan, DB
Sesar, B
Surace, JA
AF van Eyken, Julian C.
Ciardi, David R.
von Braun, Kaspar
Kane, Stephen R.
Plavchan, Peter
Bender, Chad F.
Brown, Timothy M.
Crepp, Justin R.
Fulton, Benjamin J.
Howard, Andrew W.
Howell, Steve B.
Mahadevan, Suvrath
Marcy, Geoffrey W.
Shporer, Avi
Szkody, Paula
Akeson, Rachel L.
Beichman, Charles A.
Boden, Andrew F.
Gelino, Dawn M.
Hoard, D. W.
Ramirez, Solange V.
Rebull, Luisa M.
Stauffer, John R.
Bloom, Joshua S.
Cenko, S. Bradley
Kasliwal, Mansi M.
Kulkarni, Shrinivas R.
Law, Nicholas M.
Nugent, Peter E.
Ofek, Eran O.
Poznanski, Dovi
Quimby, Robert M.
Walters, Richard
Grillmair, Carl J.
Laher, Russ
Levitan, David B.
Sesar, Branimir
Surace, Jason A.
TI THE PTF ORION PROJECT: A POSSIBLE PLANET TRANSITING A T-TAURI STAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual (25 Ori); planets and
satellites: detection; stars: individual (2MASS J05250755+0134243, CVSO
30, PTFO 8-8695, PTF1 J052507.55+013424.3); stars: pre-main sequence
ID HOBBY-EBERLY TELESCOPE; LOW-MASS STARS; RADIAL-VELOCITY VARIABILITY;
ECLIPSING BINARIES; MONITOR PROJECT; GIANT PLANETS; LIGHT CURVES; SPACED
DATA; YOUNG; SYSTEM
AB We report observations of a possible young transiting planet orbiting a previously known weak-lined T-Tauri star in the 7-10 Myr old Orion-OB1a/25-Ori region. The candidate was found as part of the Palomar Transient Factory (PTF) Orion project. It has a photometric transit period of 0.448413 +/- 0.000040 days, and appears in both 2009 and 2010 PTF data. Follow-up low-precision radial velocity (RV) observations and adaptive optics imaging suggest that the star is not an eclipsing binary, and that it is unlikely that a background source is blended with the target and mimicking the observed transit. RV observations with the Hobby-Eberly and Keck telescopes yield an RV that has the same period as the photometric event, but is offset in phase from the transit center by approximate to-0.22 periods. The amplitude (half range) of the RV variations is 2.4 kms(-1) and is comparable with the expected RV amplitude that stellar spots could induce. The RV curve is likely dominated by stellar spot modulation and provides an upper limit to the projected companion mass of M-p sin i(orb) less than or similar to 4.8 +/- 1.2 M-Jup; when combined with the orbital inclination, iorb, of the candidate planet from modeling of the transit light curve, we find an upper limit on the mass of the planetary candidate of M-p less than or similar to 5.5 +/- 1.4 M-Jup. This limit implies that the planet is orbiting close to, if not inside, its Roche limiting orbital radius, so that it may be undergoing active mass loss and evaporation.
C1 [van Eyken, Julian C.; Ciardi, David R.; von Braun, Kaspar; Kane, Stephen R.; Plavchan, Peter; Akeson, Rachel L.; Beichman, Charles A.; Gelino, Dawn M.; Ramirez, Solange V.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Bender, Chad F.; Mahadevan, Suvrath] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Bender, Chad F.; Mahadevan, Suvrath] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Brown, Timothy M.; Fulton, Benjamin J.; Shporer, Avi] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Crepp, Justin R.; Kasliwal, Mansi M.; Kulkarni, Shrinivas R.; Walters, Richard; Sesar, Branimir] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Howard, Andrew W.; Marcy, Geoffrey W.; Bloom, Joshua S.; Cenko, S. Bradley] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Boden, Andrew F.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA.
[Hoard, D. W.; Rebull, Luisa M.; Stauffer, John R.; Grillmair, Carl J.; Laher, Russ; Surace, Jason A.] CALTECH, Spitzer Sci Ctr, Jet Prop Lab, Pasadena, CA 91125 USA.
[Law, Nicholas M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Ofek, Eran O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Poznanski, Dovi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Quimby, Robert M.] Univ Tokyo, IPMU, Kashiwa, Chiba, Japan.
[Levitan, David B.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
RP van Eyken, JC (reprint author), CALTECH, NASA, Exoplanet Sci Inst, 770 S Wilson Ave,M-S 100-22, Pasadena, CA 91125 USA.
EM vaneyken@ipac.caltech.edu
RI Bender, Chad/D-4719-2012; Kane, Stephen/B-4798-2013; Howard,
Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Hoard, Donald
W./0000-0002-6800-6519; Rebull, Luisa/0000-0001-6381-515X; Ciardi,
David/0000-0002-5741-3047
FU Center for Exoplanets and Habitable Worlds; Pennsylvania State
University; Eberly College of Science; Pennsylvania Space Grant
Consortium; JPL/Caltech
FX This work was partially supported by funding from the Center for
Exoplanets and Habitable Worlds. The Center for Exoplanets and Habitable
Worlds is supported by the Pennsylvania State University, the Eberly
College of Science, and the Pennsylvania Space Grant Consortium.;
Support for this work was provided by an award issued by JPL/Caltech.
NR 69
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2012
VL 755
IS 1
AR 42
DI 10.1088/0004-637X/755/1/42
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500042
ER
PT J
AU Williams, BJ
Borkowski, KJ
Reynolds, SP
Ghavamian, P
Blair, WP
Long, KS
Sankrit, R
AF Williams, Brian J.
Borkowski, Kazimierz J.
Reynolds, Stephen P.
Ghavamian, Parviz
Blair, William P.
Long, Knox S.
Sankrit, Ravi
TI DUST IN A TYPE Ia SUPERNOVA PROGENITOR: SPITZER SPECTROSCOPY OF KEPLER'S
SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: supernova remnants; stars: AGB and post-AGB
ID LARGE-MAGELLANIC-CLOUD; GIANT BRANCH STARS; COSMIC SILICATES;
SPACE-TELESCOPE; AGB STARS; EMISSION; DESTRUCTION; GRAINS; SHOCK;
CONSTRAINTS
AB Characterization of the relatively poorly understood progenitor systems of Type Ia supernovae is of great importance in astrophysics, particularly given the important cosmological role that these supernovae play. Kepler's supernova remnant, the result of a Type Ia supernova, shows evidence for an interaction with a dense circumstellar medium (CSM), suggesting a single-degenerate progenitor system. We present 7.5-38 mu m infrared (IR) spectra of the remnant, obtained with the Spitzer Space Telescope, dominated by emission from warm dust. Broad spectral features at 10 and 18 mu m, consistent with various silicate particles, are seen throughout. These silicates were likely formed in the stellar outflow from the progenitor system during the asymptotic giant branch stage of evolution, and imply an oxygen-rich chemistry. In addition to silicate dust, a second component, possibly carbonaceous dust, is necessary to account for the short-wavelength Infrared Spectrograph and Infrared Array Camera data. This could imply a mixed chemistry in the atmosphere of the progenitor system. However, non-spherical metallic iron inclusions within silicate grains provide an alternative solution. Models of collisionally heated dust emission from fast shocks (>1000 km s(-1)) propagating into the CSM can reproduce the majority of the emission associated with non-radiative filaments, where dust temperatures are similar to 80-100 K, but fail to account for the highest temperatures detected, in excess of 150 K. We find that slower shocks (a few hundred km s(-1)) into moderate density material (n(0) similar to 50-250 cm(-3)) are the only viable source of heating for this hottest dust. We confirm the finding of an overall density gradient, with densities in the north being an order of magnitude greater than those in the south.
C1 [Williams, Brian J.; Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Williams, Brian J.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Ghavamian, Parviz] Towson Univ, Dept Phys Astron & Geosci, Towson, MD 21252 USA.
[Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Long, Knox S.] STScI, Baltimore, MD 21218 USA.
[Sankrit, Ravi] NASA, SOFIA, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Williams, BJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
EM brian.j.williams@nasa.gov
FU Spitzer Guest Observer Grant [RSA 1378040]; NASA Astrophysics Data
Analysis Program [NNX11AB14G]; [JPL-1377423]
FX We thank the anonymous referee for a careful reading of our manuscript
and many helpful discussions. This work was supported by Spitzer Guest
Observer Grant RSA 1378040 and NASA Astrophysics Data Analysis Program
Grant NNX11AB14G. W. P. B. acknowledges support from JPL-1377423 to
Johns Hopkins University.
NR 43
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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 10
PY 2012
VL 755
IS 1
AR 3
DI 10.1088/0004-637X/755/1/3
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500003
ER
PT J
AU Wuyts, E
Rigby, JR
Sharon, K
Gladders, MD
AF Wuyts, Eva
Rigby, Jane R.
Sharon, Keren
Gladders, Michael D.
TI CONSTRAINTS ON THE LOW-MASS END OF THE MASS-METALLICITY RELATION AT
z=1-2 FROM LENSED GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; gravitational lensing:
strong
ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; SIMILAR-TO 2; HIGH-REDSHIFT
GALAXIES; PHYSICAL CONDITIONS; ULTRAVIOLET-SPECTRA; STELLAR POPULATIONS;
STARBURST GALAXIES; GAS FRACTIONS; MS 1512-CB58
AB We present multi-wavelength imaging and near-IR spectroscopy for 10 gravitationally lensed galaxies at 0.9 < z < 2.5 selected from a new, large sample of strong lens systems in the Sloan Digital Sky Survey Data Release 7. We derive stellar masses from the rest-frame UV to near-IR spectral energy distributions, star formation rates (SFRs) from the dust-corrected H alpha flux, and metallicities from the [N II]/H alpha flux ratio. We combine the lensed galaxies with a sample of 60 star-forming galaxies from the literature in the same redshift range for which measurements of [N II]/H alpha have been published. Due to the lensing magnification, the lensed galaxies probe intrinsic stellar masses that are on average a factor of 11 lower than have been studied so far at these redshifts. They have specific SFRs that are an order of magnitude higher than seen for main-sequence star-forming galaxies at z similar to 2. We measure an evolution of 0.16 +/- 0.06 dex in the mass-metallicity relation between z similar to 1.4 and z similar to 2.2. In contrast to previous claims, the redshift evolution is smaller at low stellar masses. We do not see a correlation between metallicity and SFR at fixed stellar mass. The combined sample is in general agreement with the local fundamental relation between metallicity, stellar mass, and SFR from Mannucci et al. Using the Kennicutt-Schmidt law to infer gas fractions, we investigate the importance of gas inflows and outflows on the shape of the mass-metallicity relation using simple analytical models. This suggests that the Maiolino et al. calibration of the [N II]/H alpha flux ratio is biased high.
C1 [Wuyts, Eva; Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Wuyts, Eva; Sharon, Keren; Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Rigby, Jane R.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sharon, Keren] Univ Michigan, Dept Astron & Astrophys, Ann Arbor, MI 48109 USA.
RP Wuyts, E (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU Research Corporation through a Cottrell Scholars award; NASA through
JPL/Caltech; W. M. Keck Foundation
FX We thank the referee for helpful comments and suggestions and Andrey
Kravtsov and Dawn Erb for insightful discussions. M. D. G. thanks the
Research Corporation for support of this work through a Cottrell
Scholars award.; This work made use of observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Partial support for this work was provided by NASA through an
award issued by JPL/Caltech.; Data presented in this paper were partly
obtained at the W. M. Keck Observatory from telescope time allocated to
the National Aeronautics and Space Administration through the scientific
partnership with the California Institute of Technology and the
University of California. The Observatory was made possible by the
generous financial support of the W. M. Keck Foundation. We acknowledge
the very significant cultural role and reverence that the summit of
Mauna Kea has always had within the indigenous Hawaiian community. We
are most fortunate to have the opportunity to conduct observations from
this mountain.
NR 90
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Z9 36
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 AUG 10
PY 2012
VL 755
IS 1
AR 73
DI 10.1088/0004-637X/755/1/73
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 980RA
UT WOS:000306909500073
ER
PT J
AU Hand, KP
AF Hand, Kevin P.
TI The last great experiment
SO NATURE
LA English
DT Editorial Material
ID ARSENATE; GFAJ-1
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91103 USA.
RP Hand, KP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91103 USA.
EM kevin.p.hand@jpl.nasa.gov
NR 11
TC 0
Z9 0
U1 4
U2 26
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD AUG 9
PY 2012
VL 488
IS 7410
BP 160
EP 161
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 985LE
UT WOS:000307267000019
ER
PT J
AU Hamlington, BD
Leben, RR
Godin, OA
Gica, E
Titov, VV
Haines, BJ
Desai, SD
AF Hamlington, B. D.
Leben, R. R.
Godin, O. A.
Gica, E.
Titov, V. V.
Haines, B. J.
Desai, S. D.
TI Could satellite altimetry have improved early detection and warning of
the 2011 Tohoku tsunami?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB The 2011 Tohoku tsunami devastated Japan and affected coastal populations all around the Pacific Ocean. Accurate early warning of an impending tsunami requires the detection of the tsunami in the open ocean. While the lead-time was not sufficient for use in warning coastal populations in Japan, satellite altimetry observations of the tsunami could have been used to improve predictions and warnings for other affected areas. By comparing to both model results and historical satellite altimeter data, we use near-real-time satellite altimeter measurements to demonstrate the potential for detecting the 2011 Tohoku tsunami within a few hours of the tsunami being generated. We show how satellite altimeter data could be used to both directly detect tsunamis in the open ocean and also improve predictions made by models. Citation: Hamlington, B. D., R. R. Leben, O. A. Godin, E. Gica, V. V. Titov, B. J. Haines, and S. D. Desai (2012), Could satellite altimetry have improved early detection and warning of the 2011 Tohoku tsunami?, Geophys. Res. Lett., 39, L15605, doi: 10.1029/2012GL052386.
C1 [Hamlington, B. D.; Leben, R. R.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
[Hamlington, B. D.; Godin, O. A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Godin, O. A.] NOAA, Div Phys Sci, Earth Syst Res Lab, Boulder, CO USA.
[Gica, E.] Univ Washington, Joint Inst Study Atmosphere & Oceans, Seattle, WA 98195 USA.
[Gica, E.; Titov, V. V.] NOAA, NOAA Ctr Tsunami Res, PMEL, Seattle, WA USA.
[Haines, B. J.; Desai, S. D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hamlington, BD (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, 431 UCB, Boulder, CO 80309 USA.
EM hamlingt@colorado.edu
RI Godin, Oleg/E-6554-2011; Leben, Robert/F-3792-2010;
OI Godin, Oleg/0000-0003-4599-2149; Leben, Robert/0000-0003-1067-9515;
Titov, Vasily/0000-0002-1630-3829
FU NASA [NNX08AR60G]; US Navy under STTR [N06-T002]; Joint Institute for
the Study of the Atmosphere and Ocean (JISAO) under NOAA
[NA10OAR4320148]
FX This work was supported, in part, by NASA grant NNX08AR60G and the US
Navy under STTR contract N06-T002. This publication is also contribution
3798 from NOAA/Pacific Marine Environmental Laboratory and partially
funded by the Joint Institute for the Study of the Atmosphere and Ocean
(JISAO) under NOAA Cooperative Agreement NA10OAR4320148, contribution
1898. The authors thank V. G. Irisov for discussions that greatly
improved this paper.
NR 10
TC 3
Z9 3
U1 1
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 8
PY 2012
VL 39
AR L15605
DI 10.1029/2012GL052386
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 988BQ
UT WOS:000307463600001
ER
PT J
AU Ginoux, P
Prospero, JM
Gill, TE
Hsu, NC
Zhao, M
AF Ginoux, Paul
Prospero, Joseph M.
Gill, Thomas E.
Hsu, N. Christina
Zhao, Ming
TI GLOBAL-SCALE ATTRIBUTION OF ANTHROPOGENIC AND NATURAL DUST SOURCES AND
THEIR EMISSION RATES BASED ON MODIS DEEP BLUE AEROSOL PRODUCTS
SO REVIEWS OF GEOPHYSICS
LA English
DT Review
ID SOUTHWESTERN NORTH-AMERICA; AFRICAN MINERAL DUST; REGIONAL AIR-QUALITY;
SOUTHERN HIGH-PLAINS; LAST GLACIAL PERIOD; SAN-JOAQUIN VALLEY; WIND
EROSION; DESERT DUST; CLIMATE-CHANGE; OPTICAL-PROPERTIES
AB Our understanding of the global dust cycle is limited by a dearth of information about dust sources, especially small-scale features which could account for a large fraction of global emissions. Here we present a global-scale high-resolution (0.1 degrees) mapping of sources based on Moderate Resolution Imaging Spectroradiometer (MODIS) Deep Blue estimates of dust optical depth in conjunction with other data sets including land use. We ascribe dust sources to natural and anthropogenic (primarily agricultural) origins, calculate their respective contributions to emissions, and extensively compare these products against literature. Natural dust sources globally account for 75% of emissions; anthropogenic sources account for 25%. North Africa accounts for 55% of global dust emissions with only 8% being anthropogenic, mostly from the Sahel. Elsewhere, anthropogenic dust emissions can be much higher (75% in Australia). Hydro-logic dust sources (e. g., ephemeral water bodies) account for 31% worldwide; 15% of them are natural while 85% are anthropogenic. Globally, 20% of emissions are from vegetated surfaces, primarily desert shrublands and agricultural lands. Since anthropogenic dust sources are associated with land use and ephemeral water bodies, both in turn linked to the hydrological cycle, their emissions are affected by climate variability. Such changes in dust emissions can impact climate, air quality, and human health. Improved dust emission estimates will require a better mapping of threshold wind velocities, vegetation dynamics, and surface conditions (soil moisture and land use) especially in the sensitive regions identified here, as well as improved ability to address small-scale convective processes producing dust via cold pool (haboob) events frequent in monsoon regimes.
C1 [Ginoux, Paul; Zhao, Ming] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA.
[Prospero, Joseph M.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Gill, Thomas E.] Univ Texas El Paso, Environm Sci & Engn Program, El Paso, TX 79968 USA.
[Gill, Thomas E.] Univ Texas El Paso, Dept Geol Sci, El Paso, TX 79968 USA.
[Hsu, N. Christina] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ginoux, P (reprint author), NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA.
EM paul.ginoux@noaa.gov
RI Ginoux, Paul/C-2326-2008; Hsu, N. Christina/H-3420-2013; Zhao,
Ming/C-6928-2014;
OI Ginoux, Paul/0000-0003-3642-2988; Prospero, Joseph/0000-0003-3608-6160;
Gill, Thomas E/0000-0001-9011-4105
FU NOAA [NA17AE1623]; U.S. National Science Foundation [OCE 0623189, AGS
0962256]
FX The authors thank the AERONET program for establishing and maintaining
the Sun photometer sites used in this study. We are grateful to the NASA
TOMS and OMI science teams for providing the aerosol index. We are
grateful to Catherine Raphael for helping with the figures. T. E. Gill
acknowledges support via NOAA cooperative agreement NA17AE1623, and J.
M. Prospero was supported by grants from the U.S. National Science
Foundation, OCE 0623189 and AGS 0962256.
NR 215
TC 217
Z9 218
U1 9
U2 129
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 8755-1209
EI 1944-9208
J9 REV GEOPHYS
JI Rev. Geophys.
PD AUG 8
PY 2012
VL 50
AR RG3005
DI 10.1029/2012RG000388
PG 36
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 988DV
UT WOS:000307469400001
ER
PT J
AU Huang, JF
Hsu, NC
Tsay, SC
Holben, BN
Welton, EJ
Smirnov, A
Jeong, MJ
Hansell, RA
Berkoff, TA
Liu, ZY
Liu, GR
Campbell, JR
Liew, SC
Barnes, JE
AF Huang, Jingfeng
Hsu, N. Christina
Tsay, Si-Chee
Holben, Brent N.
Welton, Ellsworth J.
Smirnov, Alexander
Jeong, Myeong-Jae
Hansell, Richard A.
Berkoff, Timothy A.
Liu, Zhaoyan
Liu, Gin-Rong
Campbell, James R.
Liew, Soo Chin
Barnes, John E.
TI Evaluations of cirrus contamination and screening in ground aerosol
observations using collocated lidar systems
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID THIN CIRRUS; CLOUD CONTAMINATION; OPTICAL DEPTH; SATELLITE; ALGORITHM;
RETRIEVAL; AERONET; CLIMATOLOGY; VARIABILITY; 1.38-MU-M
AB Cirrus clouds, particularly subvisual high thin cirrus with low optical thickness, are difficult to screen in operational aerosol retrieval algorithms. Collocated aerosol and cirrus observations from ground measurements, such as the Aerosol Robotic Network (AERONET) and the Micro-Pulse Lidar Network (MPLNET), provide us with an unprecedented opportunity to systematically examine the susceptibility of operational aerosol products to cirrus contamination. Quality assured aerosol optical thickness (AOT) measurements were also tested against the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) vertical feature mask (VFM) and the Moderate Resolution Imaging Spectroradiometer (MODIS) thin cirrus screening parameters for the purpose of evaluating cirrus contamination. Key results of this study include: (1) quantitative evaluations of data uncertainties in AERONET AOT retrievals are conducted; although AERONET cirrus screening schemes are successful in removing most cirrus contamination, strong residuals displaying strong spatial and seasonal variability still exist, particularly over thin cirrus prevalent regions during cirrus peak seasons; (2) challenges in matching up different data for analysis are highlighted and corresponding solutions proposed; and (3) estimates of the relative contributions from cirrus contamination to aerosol retrievals are discussed. The results are valuable for better understanding and further improving ground aerosol measurements that are critical for aerosol-related climate research.
C1 [Huang, Jingfeng; Hsu, N. Christina; Tsay, Si-Chee; Holben, Brent N.; Welton, Ellsworth J.; Smirnov, Alexander; Hansell, Richard A.; Berkoff, Timothy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Huang, Jingfeng] Morgan State Univ, Baltimore, MD 21239 USA.
[Smirnov, Alexander] Sigma Space Corp, Lanham, MD USA.
[Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Kangnung, South Korea.
[Hansell, Richard A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Berkoff, Timothy A.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Liu, Zhaoyan] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Liu, Gin-Rong] Natl Cent Univ, Ctr Space & Remote Sensing Res, Jhongli, Taiwan.
[Campbell, James R.] USN, Res Lab, Monterey, CA USA.
[Liew, Soo Chin] Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Singapore 117548, Singapore.
[Barnes, John E.] NOAA, Mauna Loa Observ, ESRL, Hilo, HI USA.
RP Huang, JF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jingfeng.huang@noaa.gov
RI Liu, Zhaoyan/B-1783-2010; Campbell, James/C-4884-2012; Hsu, N.
Christina/H-3420-2013; Liew, Soo Chin/C-9187-2011; Huang,
Jingfeng/D-7336-2012; Tsay, Si-Chee/J-1147-2014; Hansell,
Richard/J-2065-2014
OI Liu, Zhaoyan/0000-0003-4996-5738; Campbell, James/0000-0003-0251-4550;
Liew, Soo Chin/0000-0001-8342-4682; Huang, Jingfeng/0000-0002-8779-2922;
FU NASA EOS Program; NASA Earth Observing System and Radiation Sciences
Program; NASA Earth Observing System project
FX This work is supported by grant from the NASA EOS Program, managed by
Hal Maring. Authors thank David Giles, Bo-Cai Gao, Steve Ou, Larry R.
Belcher and Zhien Wang for their constructive comments on the use of in
situ and satellite data, analysis methodology and cirrus climatology.
Aqua MODIS L1B data were obtained from NASA L1 and Atmosphere Archive
and Distribution System (LAADS). CALIPSO data were obtained from the
NASA Langley Research Center Atmospheric Science Data Center. The NASA
Micro-Pulse Lidar Network is funded by the NASA Earth Observing System
and Radiation Sciences Program. The data at the COVE site are funded by
the NASA Earth Observing System project. Authors acknowledge site PIs
Brent N. Holben, Ellsworth J. Welton, Si-Chee Tsay, Jeffrey S. Reid,
James R. Campbell, Soon-Chang Yoon, Gregory L. Schuster, Neng-Huei Lin,
Joseph M. Prospero, John E. Barnes, Soo Chin Liew and all their
colleagues for the AERONET and MPLNET sites data that are significantly
used in this paper, and all other site PIs and their colleagues for all
the site data used in this paper. Their tremendous efforts to collect
the quality data sets and put them publicly available are sincerely
appreciated. Authors thank the three reviewers for their valuable and
insightful comments that helped to improve the paper significantly.
NR 38
TC 12
Z9 12
U1 1
U2 11
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 8
PY 2012
VL 117
AR D15204
DI 10.1029/2012JD017757
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 988AG
UT WOS:000307459900001
ER
PT J
AU Drouin, B
Wiesenfeld, L
AF Drouin, Brian
Wiesenfeld, Laurent
TI Low-temperature water-hydrogen-molecule collisions probed by pressure
broadening and line shift
SO PHYSICAL REVIEW A
LA English
DT Article
ID ROTATIONAL-EXCITATION; 200 K; ICE; TRANSITION; ORTHO-H-2; PARA-H-2; H2O;
H-2
AB Theoretical H2O-H-2 pressure broadening and line shifts are compared with experimental values for three water rotational transitions. These transitions, which occur at terahertz frequencies, are primary radiant coolants for collapsing interstellar clouds that contain water. They are observed by the submillimeter/FIR Herschel space observatory. Systematic effects in previous pressure-broadening measurements that were due to ortho-hydrogen to para-hydrogen conversion have been overcome, and the present results follow the expected behavior predicted by collision theory. The systemic error, discovered through comparisons between theory and experiments, is due to conversion of ortho hydrogen to para hydrogen by water ice below 40 K. This process occurs on a time scale very short compared to astrophysical processes and may be pertinent to ice-grain interactions in the interstellar medium.
C1 [Drouin, Brian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wiesenfeld, Laurent] UJF Grenoble 1, CNRS, IPAG, UMR 5274, F-38041 Grenoble, France.
RP Drouin, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration
FX Portions of this research were carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. L.W. thanks the French
space agency CNES for travel support.
NR 27
TC 9
Z9 9
U1 3
U2 18
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD AUG 7
PY 2012
VL 86
IS 2
AR 022705
DI 10.1103/PhysRevA.86.022705
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 985LL
UT WOS:000307267800008
ER
PT J
AU Millet, DB
Apel, E
Henze, DK
Hill, J
Marshall, JD
Singh, HB
Tessum, CW
AF Millet, Dylan B.
Apel, Eric
Henze, Daven K.
Hill, Jason
Marshall, Julian D.
Singh, Hanwant B.
Tessum, Christopher W.
TI Natural and Anthropogenic Ethanol Sources in North America and Potential
Atmospheric Impacts of Ethanol Fuel Use
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID VOLATILE ORGANIC-COMPOUNDS; TROPOSPHERIC DEGRADATION; TRACE GASES;
IN-SITU; EMISSIONS; TRANSPORT; CHEMISTRY; MODEL; ACETALDEHYDE;
CONSTRAINTS
AB We used an ensemble of aircraft measurements with the GEOS-Chem chemical transport model to constrain present-day North American ethanol sources, and gauge potential long-range impacts of increased ethanol fuel use. We find that current ethanol emissions are underestimated by 50% in Western North America, and overestimated by a factor of 2 in the east. Our best estimate for year-2005 North American ethanol emissions is 670 GgC/y, with 440 GgC/y from the continental U.S. We apply these optimized source estimates to investigate two scenarios for increased ethanol fuel use in the U.S.: one that assumes a complete transition from gasoline to E85 fuel, and one tied to the biofuel requirements of the U.S. Energy Indepence and Security Act (EISA). For both scenarios, increased ethanol emissions lead to higher atmospheric acetaldehyde concentrations (by up to 14% during winter for the All-E85 scenario and 2% for the EISA scenario) and an associated shift in reactive nitrogen partitioning reflected by an increase in the peroxyacetyl nitrate (PAN) to NOy ratio. The largest relative impacts occur during fall, winter, and spring because of large natural emissions of ethanol and other organic compounds during summer. Projected changes in atmospheric PAN reflect a balance between an increased supply of peroxyacetyl radicals from acetaldehyde oxidation, and the lower NOx emissions for E85 relative to gasoline vehicles. The net effect is a general PAN increase in fall through spring, and a weak decrease over the U.S. Southeast and the Atlantic Ocean during summer. Predicted NOx concentrations decrease in surface air over North America (by as much 5% in the All-E85 scenario). Downwind of North America this effect is counteracted by higher NOx export efficiency driven by increased PAN production and transport. From the point of view of NOx export from North America, the increased PAN formation associated with E85 fuel use thus acts to offset the associated lower NOx emissions.
C1 [Millet, Dylan B.; Hill, Jason; Marshall, Julian D.; Tessum, Christopher W.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Apel, Eric] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Henze, Daven K.] Univ Colorado, Boulder, CO 80309 USA.
[Singh, Hanwant B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Millet, DB (reprint author), Univ Minnesota, Minneapolis, MN 55455 USA.
EM dbm@umn.edu
RI Chem, GEOS/C-5595-2014; Hill, Jason/A-8919-2008; Millet,
Dylan/G-5832-2012
OI Hill, Jason/0000-0001-7609-6713;
FU NASA [NNX11AB91G]; University of Minnesota Institute on the Environment:
Initiative for Renewable Energy and the Environment Grant [RL-0026-09]
FX This work was carried out in part using computing resources at the
University of Minnesota Supercomputing Institute. We thank Alex Guenther
for his helpful input. D.K.H. recognizes support from NASA Grant
NNX11AB91G. J.H., J.D.M., and C.W.T. recognize support from the
University of Minnesota Institute on the Environment: Initiative for
Renewable Energy and the Environment Grant RL-0026-09.
NR 55
TC 12
Z9 12
U1 3
U2 45
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD AUG 7
PY 2012
VL 46
IS 15
BP 8484
EP 8492
DI 10.1021/es300162u
PG 9
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 984OG
UT WOS:000307199800072
PM 22731385
ER
PT J
AU Brecht, AS
Bougher, SW
AF Brecht, A. S.
Bougher, S. W.
TI Dayside thermal structure of Venus' upper atmosphere characterized by a
global model
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MU-M WAVELENGTH; SPECTRAL-LINE OBSERVATIONS; GENERAL-CIRCULATION MODEL;
HETERODYNE SPECTROSCOPY; LOWER THERMOSPHERE; INFRARED OBSERVATIONS;
DIURNAL-VARIATIONS; MIDDLE ATMOSPHERE; WIND VELOCITIES; ATOMIC OXYGEN
AB Observations of Venus' dayside thermal structure are being conducted through ground based observatories. These temperature measurements, along with those from several instruments onboard the current Venus Express mission, are augmenting the previous thermal structure data from past missions (e.g., Veneras', Pioneer Venus Orbiter, Pioneer Venus Probes). These recent ground-based and VEx observations reveal the Venus dayside lower thermosphere to be considerably warmer and dynamically important than previously understood. In this study, a three dimensional general circulation model, the Venus Thermospheric General Circulation Model (VTGCM), is used to provide dayside temperature predictions for comparison to these recent ground based observations. Such a comparison serves to identify and quantify the underlying thermal processes responsible for the observed dayside temperature structure. The VTGCM reproduces the dayside temperatures observed near 110 km at noon from 40 degrees S to 40 degrees N very well. In addition, the global winds generated by these warm dayside temperatures are shown to give rise to dayside upwelling (divergence) and nightside subsidence (convergence) resulting in nightside warming near the anti-solar point at similar to 104 km. Corresponding nightside temperatures reach similar to 198 K, in accord with averaged measurements. This agreement implies (1) it is important for GCMs to include the updated radiative heating and cooling rates presented in Roldan et al. (2000) and (2) the current VTS3 and VIRA empirical models are in-sufficient in representing the warm regions observed in the thermal structure of the dayside lower thermosphere (similar to 100 to 130 km) and need to be updated.
C1 [Brecht, A. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bougher, S. W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Brecht, AS (reprint author), NASA, Ames Res Ctr, MSC 245-3, Moffett Field, CA 94035 USA.
EM amanda.s.brecht@nasa.gov
RI Bougher, Stephen/C-1913-2013
OI Bougher, Stephen/0000-0002-4178-2729
FU NASA's Postdoctoral Program at the Ames Research Center; NASA; SwRI
[B99073JD]; NSF [AST-0406650]; National Science Foundation; NASA
High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center
FX The authors want to thank C. Lee, M. Lopez-Valverde, R. T. Clancy, and
C. D. Parkinson for useful discussions concerning this research. Brecht
is supported by NASA's Postdoctoral Program at the Ames Research Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. Bougher acknowledges NASA Venus Express Participating
Scientist support via SwRI subcontract B99073JD. NSF grant AST-0406650
also sponsored a portion of this research. Computer resources were
supplied by both the National Center for Atmospheric Research, which is
sponsored by the National Science Foundation, and NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center.
NR 73
TC 9
Z9 9
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD AUG 7
PY 2012
VL 117
AR E08002
DI 10.1029/2012JE004079
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 988DH
UT WOS:000307467900001
ER
PT J
AU Li, W
Thorne, R
Bortnik, J
McPherron, R
Nishimura, Y
Angelopoulos, V
Richardson, IG
AF Li, Wen
Thorne, Richard
Bortnik, Jacob
McPherron, Robert
Nishimura, Yukitoshi
Angelopoulos, Vassilis
Richardson, Ian G.
TI Evolution of chorus waves and their source electrons during storms
driven by corotating interaction regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; INTERPLANETARY MAGNETIC-FIELD; RADIATION BELT
ELECTRONS; GEOMAGNETIC-ACTIVITY; RELATIVISTIC ELECTRONS; SOLAR-WIND;
GEOSYNCHRONOUS ORBIT; SEMIANNUAL VARIATION; STREAM INTERFACES; THEMIS
AB During Corotating Interaction Region (CIR)-driven storms, relativistic electron fluxes in the outer radiation belt decrease in the main phase, followed by a gradual increase in the recovery phase. Recent studies have shown that whistler mode chorus waves play an important role in accelerating the seed electron population to relativistic energies in the outer radiation belt. However, the evolution of chorus waves and their source electrons responsible for the wave excitation during storm various phases is not well understood. In this study we select 72 CIR-driven storm periods over the interval 2007-2011 to perform superposed epoch analysis of the evolution of chorus waves and source electrons in the L* and MLT range extensively observed by THEMIS during various phases of CIR-driven storms. The wave amplitudes and the occurrence of chorus waves substantially increase and peak in the main phase and gradually decrease in the following recovery phase at L* < similar to 7. The phase space density of source electrons at L* < similar to 7 also increases in the main phase followed by a gradual decay in the recovery phase, showing a remarkable consistency with the evolution of chorus waves. Importantly, the evolution of the chorus wave activity and source electron population is highly dependent on the preceding interplanetary magnetic field (IMF) B-z orientation. Our results suggest that the increased activity of chorus waves and source electrons may contribute to the enhanced radiation belt electron flux in the recovery phase of CIR-driven storms, but an additional mechanism is probably required to explain the main phase dropout.
C1 [Li, Wen; Thorne, Richard; Bortnik, Jacob; Nishimura, Yukitoshi] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[McPherron, Robert; Angelopoulos, Vassilis] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Richardson, Ian G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Richardson, Ian G.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
RP Li, W (reprint author), Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
EM moonli@atmos.ucla.edu
RI Li, Wen/F-3722-2011;
OI Richardson, Ian/0000-0002-3855-3634
FU NASA [NNX11AD75G, NNX11AR64G, NNX10AE61G]; NSF [ATM 0802843,
AGS-0840178]; NASA contract [NAS5-02099]; German Ministry for Economy
and Technology; German Center for Aviation and Space (DLR) [50 OC 0302]
FX We acknowledge NASA grants NNX11AD75G, NNX11AR64G, NNX10AE61G and NSF
grants ATM 0802843 and AGS-0840178. The authors acknowledge NASA
contract NAS5-02099 for the use of data from the THEMIS Mission.
Specifically, we thank O. Le Contel and A. Roux for use of SCM data; J.
W. Bonnell and F. S. Mozer for use of EFI data; and K. H. Glassmeier, U.
Auster, and W. Baumjohann for the use of FGM data provided under the
lead of the Technical University of Braunschweig and with financial
support through the German Ministry for Economy and Technology and the
German Center for Aviation and Space (DLR) under contract 50 OC 0302.
The authors thank the ONERA library for providing the tools to calculate
L*, the World Data Center for Geomagnetism, Kyoto for providing AE, Kp
and Sym-H indices, and the Space Physics Data Facility at the NASA
Goddard Space Flight Center for providing the OMNI2 data.
NR 82
TC 8
Z9 8
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 7
PY 2012
VL 117
AR A08209
DI 10.1029/2012JA017797
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 987ZX
UT WOS:000307459000002
ER
PT J
AU Aasi, J
Abadie, J
Abbott, BP
Abbott, R
Abbott, TD
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Acernese, F
Adams, C
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TI The characterization of Virgo data and its impact on gravitational-wave
searches
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID SPIN-DOWN LIMIT; PERIODIC SOURCES; SCIENCE RUN; RADIATION; NOISE;
INTERFEROMETER; EMISSION; PULSARS; PHASE
AB Between 2007 and 2010 Virgo collected data in coincidence with the LIGO and GEO gravitational-wave (GW) detectors. These data have been searched for GWs emitted by cataclysmic phenomena in the universe, by non-axisymmetric rotating neutron stars or from a stochastic background in the frequency band of the detectors. The sensitivity of GW searches is limited by noise produced by the detector or its environment. It is therefore crucial to characterize the various noise sources in a GW detector. This paper reviews the Virgo detector noise sources, noise propagation, and conversion mechanisms which were identified in the three first Virgo observing runs. In many cases, these investigations allowed us to mitigate noise sources in the detector, or to selectively flag noise events and discard them from the data. We present examples from the joint LIGO-GEO-Virgo GW searches to show how well noise transients and narrow spectral lines have been identified and excluded from the Virgo data. We also discuss how detector characterization can improve the astrophysical reach of GW searches.
C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allocca, A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C. B.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chalermsongsak, T.; Corsi, A.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Doravari, S.; Driggers, J. C.; Ehrens, P.; Engel, R.; Etzel, T.; Fotopoulos, N.; Gustafson, E. K.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Lindquist, P. E.; Litvine, V.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Pedraza, M.; Phelps, M.; Poux, C.; Price, L. R.; Privitera, S.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Santamaria, L.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C. I.; Vass, S.; Villar, A. E.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Abbott, T. D.; Griffo, C.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
[Abernathy, M.; Barr, B.; Bassiri, R.; Bastarrika, M.; Bell, A. S.; Bell, C.; Beveridge, N.; Campsie, P.; Cumming, A.; Cunningham, L.; Edgar, M.; Evans, K.; Gill, C.; Grant, A.; Hammond, G.; Haughian, K.; Hendry, M. A.; Heng, I. S.; Hild, S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Logue, J.; Macarthur, J.; Macdonald, E.; Martin, I. W.; Murray, P. G.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reed, S.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Speirits, F. C.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Accadia, T.; Bebronne, M.; Buskulic, D.; Dietz, A.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Tournefier, E.; Verkindt, D.; Yvert, M.] Univ Savoie, Lab Annecy Le Vieux Phys Particules LAPP, CNRS, IN2P3, F-74941 Annecy Le Vieux, France.
[Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Forte, L. A.; Garufi, F.; Mosca, S.; Parisi, M.; Persichetti, G.; Romano, R.] Ist Nazl Fis Nucl, Sez Napolia, I-80126 Naples, Italy.
Univ Naples Federico II, I-80126 Naples, Italy.
[Acernese, F.; Barone, F.; Romano, R.] Complesso Univ Monte S Angelo, I-80126 Naples, Italy.
[Adams, C.; Allocca, A.; Aston, S. M.; Betzwieser, J.; Birch, J.; Bridges, D. O.; Cowart, M.; Di Virgilio, A.; Evans, T.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Heintze, M. C.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Le Roux, A.; Lormand, M.; Meyer, M. S.; Nolting, D.; O'Reilly, B.; Overmier, H.; Ramet, C.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thorne, K. A.; Traylor, G.; Welborn, T.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Adams, T.; Dent, T.; Edwards, M.; Fairhurst, S.; Hanna, C.; Macleod, D. M.; Messenger, C.; Nuttall, L.; Predoi, V.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Veitch, J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Affeldt, C.; Allen, B.; Allocca, A.; Ast, S.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Damjanic, M.; Danzmann, K.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Heurs, M.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Lastzka, N.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Shaltev, M.; Simakov, D.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Thuering, A.; Vahlbruch, H.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkelmann, L.; Winkler, W.; Wittel, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Affeldt, C.; Allen, B.; Ast, S.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Damjanic, M.; Danzmann, K.; Di Palma, I.; Di Virgilio, A.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Heurs, M.; Hewitson, M.; Ivanov, A.; Kaufer, H.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Lastzka, N.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mullavey, A.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Sergeev, A.; Shaltev, M.; Simakov, D.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Thuering, A.; Vahlbruch, H.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkelmann, L.; Winkler, W.; Wittel, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Agathos, M.; Bauera, Th S.; Beker, M. G.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Jonker, R. J. G.; Li, T. G. F.; Rabeling, D. S.; ter Braacka, A. P. M.; van den Brandab, J. F. J.; Van den Broeck, C.; van der Putten, S.; Vitale, S.] Nikhef, Amsterdam, Netherlands.
[Bulten, H. J.; Rabeling, D. S.; van den Brandab, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Agatsuma, K.; Fujimoto, M-K; Hayama, K.; Izumi, K.; Kawamura, S.; Mori, T.; Nishizawa, A.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Allen, B.; Allocca, A.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Di Virgilio, A.; Favata, M.; Giampanis, S.; Hammer, D.; Hughey, B.; Kline, J.; Koranda, S.; Mercer, R. A.; Moe, B.; Ochsner, E.; Oldenberg, R. G.; O'Shaughnessy, R.; Pankow, C.; Papa, M. A.; Siemens, X.; Skelton, G. R.; Wade, L.; Wade, M.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allocca, A.; Bastiab, A.; Bitossi, M.; Bonelli, L.; Boschi, V.; Braccini, S.; Bradaschia, C.; Cella, G.; Colacino, C. N.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Giazotto, A.; Mantovani, M.; Paoletti, F.; Paoletti, R.; Passaquieti, R.; Passuello, D.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Torrea, O.; Vajente, G.] Ist Nazl Fis Nucl, Sez Pisa, Pisa, Italy.
[Bastiab, A.; Bonelli, L.; Colacino, C. N.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56127 Pisa, Italy.
[Allocca, A.; Paoletti, R.; Torrea, O.] Univ Siena, I-53100 Siena, Italy.
[Amariutei, D.; Bao, Y.; Ciani, G.; Feldbaum, D.; Gleason, J.; Hartman, M. T.; Klimenko, S.; Liu, Z.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Tanner, D. B.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Colla, A.; Conte, A.; Frasca, S.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Atkinson, D.; Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Bland, B.; Clara, F.; Cook, D.; Di Virgilio, A.; Garcia, J.; Gray, C.; Hanks, J.; Ingram, D. R.; Ivanov, A.; Kawabe, K.; Landry, M.; Lhuillier, V.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R. L.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Aylott, B. E.; Bond, C.; Carbone, L.; Cruise, A. M.; Cutler, R. M.; Freise, A.; Fulda, P. J.; Grover, K.; Hallam, J. M.; Lodhia, D.; Mandel, I.; Mingarelli, C. M. F.; Page, A.; Sidery, T. L.; Smith, R. J. E.; Vecchio, A.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Babak, S.; Behnke, B.; Grunewald, S.; Krishnan, B.; Leaci, P.; Papa, M. A.; Robinson, E. L.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Baker, P.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA.
[Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cuoco, E.; Dattilo, V.; Day, R.; Ferrini, F.; Fiori, I.; Genin, E.; Hemming, G.; Kasprzack, M.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Ruggi, P.; Sentenac, D.; Swinkels, B.; Tacca, M.] European Gravitat Observ EGO, I-56021 Cascina, PI, Italy.
[Ballmer, S.; Brown, D. A.; Couvares, P.; Fisher, R. P.; Harry, I. W.; Kelley, D.; Kumar, P.; Lough, J.; Nitz, A.; Perreca, A.; Saulson, P. R.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barsotti, L.; Bodiya, T. P.; Corbitt, T. R.; Donovan, F.; Dwyer, S.; Evans, M.; Foley, S.; Fritschel, P.; Katsavounidis, E.; Kissel, J. S.; Kwee, P.; MacInnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Oelker, E.; Sankar, S.; Shapiro, B.; Shoemaker, D. H.; Smith-Lefebvre, N. D.; Vaulin, R.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA.
[Barsuglia, M.; Bouhou, B.; Buy, C.; Chassande-Mottin, E.; Ward, R. L.] Univ Paris Diderot, Observ Paris, APC, CNRS,IN2P3,CEA Irfu, Paris 13, France.
[Bartos, I.; Belopolski, I.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D.; Raffai, P.; Tse, M.] Columbia Univ, New York, NY 10027 USA.
[Bassiri, R.; Beck, D.; Bhadbade, T.; Byer, R. L.; Clark, D. E.; DeBbra, D.; Herrera, V.; Kim, N.; Kurdyumov, R.; Lantz, B.; Markosyan, A.; Roberts, M.] Stanford Univ, Stanford, CA 94305 USA.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Bejgerc, M.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland.
[Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Benacquista, M.; Biswas, R.; Cagnoli, G.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Stroeer, A. S.; Torres, C. V.] Univ Texas Brownsville, Brownsville, TX 78520 USA.
[Beyersdorf, P. T.; Cordier, M.] San Jose State Univ, San Jose, CA 95192 USA.
[Bilenko, I. A.; Braginsky, V. B.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L. G.; Strigin, S. E.; Vyatchanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia.
[Bizouard, M. A.; Brisson, V.; Cavalier, F.; Davier, M.; Franco, S.; Hello, P.; Kasprzack, M.; Leroya, N.; Robinet, F.; Vavoulidis, M.; Was, M.] Univ Paris 11, LAL, CNRS, IN2P3, F-91898 Orsay, France.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Blackburn, L.; Camp, J. B.; Kanner, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blair, D.; Chen, X.; Chung, S.; Coward, D. M.; Danilishin, S. L.; Di Virgilio, A.; Dumas, J-C; Hooper, S.; Howell, E. J.; Ivanov, A.; Ju, L.; Susmithan, S.; Wen, L.; Whitcomb, S. E.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia.
[Bondarescu, R.; Finn, L. S.; Menendez, D. F.; Owen, B. J.; Titsler, C.] Penn State Univ, University Pk, PA 16802 USA.
[Brillet, A.; Cleva, F.; Coulon, J-P; Fournier, J-D; Heitmann, H.; Man, N.; Pichot, M.; Regimbaua, T.; Vinet, J-Y] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France.
[Bondu, F.; Hayau, J-F] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France.
[Bonnand, R.; Cagnoli, G.; Degallaix, J.; Flaminio, R.; Franc, J.; Galimberti, M.; Granata, M.; Michel, C.; Morgado, N.; Pinard, L.; Saracco, E.; Sassolas, B.] CNRS, LMA, IN2P3, F-69622 Villeurbanne, France.
[Bose, S.; Dayanga, T.; Ghosh, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA.
[Bosia, L.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Gammaitoni, L.; Neri, I.; Travasso, F.] Univ Perugia, I-06123 Perugia, Italy.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[Branchesi, M.; Guidi, G. M.; Lorenzini, M.; Losurdoa, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Sesto Fiorentino, Italy.
[Branchesi, M.; Cesarini, E.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino, I-61029 Urbino, Italy.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Leonor, I.; Quitzow-James, R.; Schofield, R. M. S.] Univ Oregon, Eugene, OR 97403 USA.
[Briant, T.; Cohadon, P-F; Heidmann, A.] Univ Paris 06, UPMC, Lab Kastler Brossel, ENS,CNRS, F-75005 Paris, France.
[Buonanno, A.; Capano, C. D.; Kanner, J. B.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
[Burguet-Castell, J.; Gil-Casanova, S.; Husa, S.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma De Mallorca, Spain.
[Cadonati, L.; Clark, J. A.; Hoak, D.; McIver, J.; Mohapatra, S. R. P.] Univ Massachusetts, Amherst, MA 01003 USA.
[Cannon, K.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Chen, W.; Du, Z.; Li, J.; Liu, Y.; Wan, Y.; Wang, X.; Zhang, F.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Cavaglia, M.; Dietz, A.; Rankins, B.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Cavaglia, M.; Dietz, A.; Rankins, B.] Univ Mississippi, University, MS 38677 USA.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, Y.; Hong, T.; Kaufman, K.; Miao, H.; Ott, C. D.; Somiya, K.; Thorne, K. S.; Wen, L.; Yang, H.] Caltech CaRT, Pasadena, CA 91125 USA.
[Chincarini, A.; Gemme, G.; Prato, M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Cho, H. S.; Kim, Y. M.; Lee, C. H.] Pusan Natl Univ, Pusan 609735, South Korea.
[Chow, J.; Chua, S. S. Y.; Inta, R.; Lam, P. K.; McClelland, D. E.; Miller, J.; Mow-Lowry, C. M.; Mullavey, A.; Nguyen, T.; Scott, S. M.; Shaddock, D. A.; Slagmolen, B. J. J.; Stefszky, M.; Wade, A.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Ballinger, T.; Christensen, N.; Coughlin, M.; Hardt, A.; Isogai, T.; Tucker, E.] Carleton Coll, Northfield, MN 55057 USA.
[Chung, C. T. Y.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Allocca, A.; Coccia, E.; D'Antonio, S.; Emilio, M. Di Paolo; Fafone, V.; Minenkov, Y.; Morgia, A.; Palladino, L.; Re, V.; Rocchi, A.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Rome, Italy.
[Coccia, E.; Fafone, V.; Morgia, A.; Re, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Emilio, M. Di Paolo; Palladino, L.] Univ Aquila, I-67100 Laquila, Italy.
[Addesso, P.; Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy.
[Costa, C. A.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil.
[Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; Endroczi, G.; Gaspar, M. E.; Racz, I.; Vasuth, M.] RMKI, Wigner RCP, H-1121 Budapest, Hungary.
[Dhurandhar, S.; Gupta, R.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Dorsher, S.; Kandhasamy, S.; Mandic, V.; Pihlaja, M.; Prestegard, T.; Thrane, E.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Drago, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Trento, Italy.
[Yamamoto, K.] Univ Trent, I-38050 Trento, Italy.
[Taffarello, L.; Vedovato, G.; Zendri, J-P] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
Univ Padua, I-35131 Padua, Italy.
[Drever, R. W. P.; Harms, J.; Langley, A.] CALTECH, Pasadena, CA 91125 USA.
[Farr, B. F.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Raymond, V.; Rodriguez, C.; Yablon, J.] Northwestern Univ, Evanston, IL 60208 USA.
[Frei, M. A.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Frei, Z.; Gelencser, G.; Raffai, P.; Szeifert, G.] Eotvos Lorand Univ, H-1117 Budapest, Hungary.
[Gair, J.; Graff, P. B.] Univ Cambridge, Cambridge CB2 1TN, England.
[Gergely, L. A.; Keresztes, Z.] Univ Szeged, H-6720 Szeged, Hungary.
[Greenhalgh, R. J. S.; O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Jesse, E.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Hanna, C.] Perimeter Inst Theoret Phys, Toronto, ON N2L 2Y5, Canada.
[Harry, G. M.] American Univ, Washington, DC 20016 USA.
[Holtrop, M.] Univ New Hampshire, Durham, NH 03824 USA.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Kang, G.; Kim, B. K.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Kasturi, R.; Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, C.] Lund Observ, SE-22100 Lund, Sweden.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[McGuire, S. C.] So Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA.
[Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA.
[Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Oh, J. J.; Oh, S. H.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Santostasi, G.] McNeese State Univ, Lake Charles, LA 70609 USA.
[Summerscales, T. Z.; Ugolini, D.] Andrews Univ, Berrien Springs, MI 49104 USA.
Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
EM robinet@lal.in2p3.fr
RI Ward, Robert/I-8032-2014; Ferrante, Isidoro/F-1017-2012; Prato,
Mirko/D-8531-2012; Travasso, Flavio/J-9595-2016; Bartos,
Imre/A-2592-2017; Cella, Giancarlo/A-9946-2012; Cesarini,
Elisabetta/C-4507-2017; Chow, Jong/A-3183-2008; Frey,
Raymond/E-2830-2016; Di Virgilio, Angela Dora Vittoria/E-9078-2015;
Sergeev, Alexander/F-3027-2017; Rocchi, Alessio/O-9499-2015; Martelli,
Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring,
Tobias/A-8596-2016; Howell, Eric/H-5072-2014; Heidmann,
Antoine/G-4295-2016; Bao, Yiliang/G-9848-2016; Ott,
Christian/G-2651-2011; Biswas, Rahul/H-7474-2016; mosca,
simona/I-7116-2012; Frasconi, Franco/K-1068-2016; Pinto,
Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Khalili,
Farit/D-8113-2012; McClelland, David/E-6765-2010; Vecchio,
Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Finn, Lee
Samuel/A-3452-2009; Sigg, Daniel/I-4308-2015; Tacca, Matteo/J-1599-2015;
Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Neri, Igor/F-1482-2010; Shaddock, Daniel/A-7534-2011;
Postiglione, Fabio/O-4744-2015; Steinlechner, Sebastian/D-5781-2013;
Drago, Marco/E-7134-2013; Re, Virginia /F-6403-2013; Hild,
Stefan/A-3864-2010; Martin, Iain/A-2445-2010; Pitkin,
Matthew/I-3802-2013; Gammaitoni, Luca/B-5375-2009; Miao,
Haixing/O-1300-2013; Khazanov, Efim/B-6643-2014; Salemi,
Francesco/F-6988-2014; Nelson, John/H-7215-2014; Danilishin,
Stefan/K-7262-2012; Canuel, Benjamin/C-7459-2014; Lee,
Chang-Hwan/B-3096-2015; Vyatchanin, Sergey/J-2238-2012; Puppo,
Paola/J-4250-2012; Colla, Alberto/J-4694-2012; Rapagnani,
Piero/J-4783-2012; CONTE, ANDREA/J-6667-2012; Gemme,
Gianluca/C-7233-2008; Bilenko, Igor/D-5172-2012; Allen,
Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Strain,
Kenneth/D-5236-2011; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013;
Lam, Ping Koy/A-5276-2008; Parisi, Maria/D-2817-2013; Santamaria,
Lucia/A-7269-2012; Marchesoni, Fabio/A-1920-2008; prodi,
giovanni/B-4398-2010; Costa, Cesar/G-7588-2012; Bell, Angus/E-7312-2011;
Prokhorov, Leonid/I-2953-2012; Vicere, Andrea/J-1742-2012; Ciani,
Giacomo/G-1036-2011; Mitrofanov, Valery/D-8501-2012; Gorodetsky,
Michael/C-5938-2008; Punturo, Michele/I-3995-2012; Strigin,
Sergey/I-8337-2012; Cuoco, Elena/I-8789-2012;
OI Coccia, Eugenio/0000-0002-6669-5787; Hallam, Jonathan
Mark/0000-0002-7087-0461; Vetrano, Flavio/0000-0002-7523-4296; Addesso,
Paolo/0000-0003-0895-184X; Naticchioni, Luca/0000-0003-2918-0730;
Nishizawa, Atsushi/0000-0003-3562-0990; calloni,
enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Husa,
Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298;
Vocca, Helios/0000-0002-1200-3917; Pinto, Innocenzo
M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Swinkels,
Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870;
Santamaria, Lucia/0000-0002-5986-0449; Pierro,
Vincenzo/0000-0002-6020-5521; Drago, Marco/0000-0002-3738-2431; Ward,
Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan,
John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320;
Fairhurst, Stephen/0000-0001-8480-1961; Boschi,
Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418;
Ferrante, Isidoro/0000-0002-0083-7228; Prato, Mirko/0000-0002-2188-8059;
Travasso, Flavio/0000-0002-4653-6156; Cella,
Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167;
Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Di
Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Jaranowski,
Piotr/0000-0001-8085-3414; Aulbert, Carsten/0000-0002-1481-8319; Milano,
Leopoldo/0000-0001-9487-5876; Veitch, John/0000-0002-6508-0713;
Principe, Maria/0000-0002-6327-0628; Kanner, Jonah/0000-0001-8115-0577;
Rocchi, Alessio/0000-0002-1382-9016; Martelli,
Filippo/0000-0003-3761-8616; Gehring, Tobias/0000-0002-4311-2593;
Howell, Eric/0000-0001-7891-2817; Heidmann, Antoine/0000-0002-0784-5175;
Ott, Christian/0000-0003-4993-2055; Biswas, Rahul/0000-0002-0774-8906;
mosca, simona/0000-0001-7869-8275; Frasconi, Franco/0000-0003-4204-6587;
McClelland, David/0000-0001-6210-5842; Vecchio,
Alberto/0000-0002-6254-1617; Finn, Lee Samuel/0000-0002-3937-0688; Sigg,
Daniel/0000-0003-4606-6526; Tacca, Matteo/0000-0003-1353-0441; Graef,
Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Neri,
Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494;
Postiglione, Fabio/0000-0003-0628-3796; Steinlechner,
Sebastian/0000-0003-4710-8548; Pitkin, Matthew/0000-0003-4548-526X;
Gammaitoni, Luca/0000-0002-4972-7062; Miao, Haixing/0000-0003-4101-9958;
Nelson, John/0000-0002-6928-617X; Danilishin,
Stefan/0000-0001-7758-7493; Lee, Chang-Hwan/0000-0003-3221-1171; Puppo,
Paola/0000-0003-4677-5015; Gemme, Gianluca/0000-0002-1127-7406; Allen,
Bruce/0000-0003-4285-6256; Strain, Kenneth/0000-0002-2066-5355; Zhao,
Chunnong/0000-0001-5825-2401; Lam, Ping Koy/0000-0002-4421-601X;
Marchesoni, Fabio/0000-0001-9240-6793; prodi,
giovanni/0000-0001-5256-915X; Bell, Angus/0000-0003-1523-0821; Vicere,
Andrea/0000-0003-0624-6231; Ciani, Giacomo/0000-0003-4258-9338;
Gorodetsky, Michael/0000-0002-5159-2742; Punturo,
Michele/0000-0001-8722-4485; Di Paolo Emilio,
Maurizio/0000-0002-9558-3610; Vitale, Salvatore/0000-0003-2700-0767;
PERSICHETTI, GIANLUCA/0000-0001-8424-9791; Freise,
Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587;
Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard
F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Sorazu,
Borja/0000-0002-6178-3198; Bondu, Francois/0000-0001-6487-5197; Zweizig,
John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030;
O'Shaughnessy, Richard/0000-0001-5832-8517; Granata,
Massimo/0000-0003-3275-1186
FU United States National Science Foundation; Science and Technology
Facilities Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany; Australian Research Council; International
Science Linkages program of the Commonwealth of Australia; Council of
Scientific and Industrial Research of India; Istituto Nazionale di
Fisica Nucleare of Italy; Spanish Ministerio de Economia y
Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern
de les Illes Balears; Netherlands Organisation for Scientific Research;
Polish Ministry of Science and Higher Education; FOCUS Programme of
Foundation for Polish Science; Royal Society; Scottish Funding Council;
Scottish Universities Physics Alliance; National Aeronautics and Space
Administration; Carnegie Trust; Leverhulme Trust; David and Lucile
Packard Foundation; Research Corporation; Alfred P Sloan Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation for the construction and operation of the
LIGO Laboratory, the Science and Technology Facilities Council of the
United Kingdom, the Max-Planck-Society, and the State of
Niedersachsen/Germany for support of the construction and operation of
the GEO600 detector, and the Italian Istituto Nazionale di Fisica
Nucleare and the French Centre National de la Recherche Scientifique for
the construction and operation of the Virgo detector. The authors also
gratefully acknowledge the support of the research by these agencies and
by the Australian Research Council, the International Science Linkages
program of the Commonwealth of Australia, the Council of Scientific and
Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
of Italy, the Spanish Ministerio de Economia y Competitividad, the
Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes
Balears, the Foundation for Fundamental Research on Matter supported by
the Netherlands Organisation for Scientific Research, the Polish
Ministry of Science and Higher Education, the FOCUS Programme of
Foundation for Polish Science, the Royal Society, the Scottish Funding
Council, the Scottish Universities Physics Alliance, The National
Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme
Trust, the David and Lucile Packard Foundation, the Research
Corporation, and the Alfred P Sloan Foundation.
NR 79
TC 37
Z9 37
U1 4
U2 58
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD AUG 7
PY 2012
VL 29
IS 15
AR 155002
DI 10.1088/0264-9381/29/15/155002
PG 41
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 974GU
UT WOS:000306421400003
ER
PT J
AU Cervini-Silva, J
Kearns, J
Banfield, J
AF Cervini-Silva, Javiera
Kearns, Josh
Banfield, Jillian
TI Steady-state dissolution kinetics of mineral ferric phosphate in the
presence of desferrioxamine-B and oxalate ligands at pH=4-6 and T=24 +/-
0.6 degrees C
SO CHEMICAL GEOLOGY
LA English
DT Article
DE Siderophore; Microbial dissolution; Phosphorous; Ligand competition
ID SIDEROPHORE-PROMOTED DISSOLUTION; GOETHITE DISSOLUTION; LAKE OKEECHOBEE;
PLANT-GROWTH; IRON; SOIL; PH; STRENGITE; TRIHYDROXAMATE; (HYDR)OXIDES
AB Ferric phosphate (FePO4 center dot 2H(2)O) is one of the most common secondary phosphate minerals in the environment. Nevertheless, few studies address the biological dissolution mechanism(s) of FePO4 center dot 2H(2)O. This paper reports steady-state dissolution rates of synthetic FePO4 center dot 2H(2)O at 4 <= pH(0)<= 6 by desferrioxamine-B (DFO-B) and oxalate (Ox) ligands. The composition of the influent solution was 10 mM NaCIO4, 5 mM MES buffer. The influent solution was adjusted to 4 <= pH(0)<= 6 by adding aliquots of HNO3 or NaOH stock solution. The initial concentrations of DFO-B and Ox, [DFO-B](0) and [Ox](0), ranged from 0 to 135 mu M, and 0 to 345 mu M. Geochemical thermodynamic equilibrium modeling was conducted using MINEQL(+) (Schecher and McAvoy, 1998). Speciation calculations were based on thermodynamic formation constants at 298.17 K, K-298 (infinite dilution reference state). Ligand-promoted dissolution rates were determined after steady-state values. Iron concentrations in the effluent solution were quantified (t>500 h). Typical effluent-flow rate was maintained at 0.10 +/- 0.01 mL min(-1). The measured dissolution rate of FePO4 center dot 2H(2)O by DFO-B and Ox, R-DFO-Ox(Obs), was compared to the sum of dissolution rates by DFO-B (RDFO-B) or Ox (R-Ox), R-DFO-Ox(Sum) (R-DFO-Ox(Sum) = RDFO-B + R-Ox). Results were analyzed using the t student test. Obtained data values with p <= 0.05 (*) and <= 0.01 (**) were considered to differ statistically from control experiments. Dissolution rates by DFO-B (RDFO-B) increased with [DFOB](0), and no evidence of surface masking became apparent. By contrast, dissolution rates by Ox (R-Ox) varied with [Ox](0) and pHo. The kinetics of dissolution by Ox was not explained by a first-order mineral dissolution behavior. Dissolution rates by DFO-B and Ox (R-DFO-Ox(Obs)) surpassed RDFO-B or R-Ox, and increased with proton activity. Reacting FePO4 center dot 2H(2)O with DFO-B and high amounts of Ox resulted in higher values for R-DFO-Ox(Obs) relative to RDFO-B. Observed (R-DFO-Ox(Obs)) to calculated (R-DFO-Ox(Sum) = RDFO-B + R-Ox) ratio was found to be highest at [DFOB](0)= 50 mu M and [Ox](0) = 49 mu M. Increases in the proton activity favors the dissolution of FePO4 center dot 2H(2)O by DFO-B and Ox, explained because the sequestration of Fe(III) at the surface vicinity in the form of adsorbed Fe( III)-oxalate complexes. A direct comparison between the dissolution behavior of FePO4 center dot 2H(2)O by DFO-B and Ox against those for goethite (alpha-FeOOH) and Al goethite (AlFeOOH) was conducted. The dissolution behavior was found to be a function of the mineral structure. RDFO-B values for FePO4 center dot 2H(2)O by 22.5 mu M DFO-B surpassed those for alpha-FeOOH or alpha-AlFeOOH by 20 mu M DFO-B, namely, 37, and 11.6 and 3-5 mu mol kg(-1) h(-1), respectively. Rox values for FePO4 center dot 2H(2)O by 49 mM Ox surpassed that for alpha-FeOOH by 70 mu M Ox or alpha-AlFeOOH by 50 mu M Ox, namely, i.e., 12, and 0.7 and 0.
1 mu mol kg(-1) h(-1). The latter results agree with the idea of the inhibition of Fe release in goethite because its sequestration in the form of adsorbed Fe(III) oxalate complexes. In contrast, a different scenario holds true for dissolution by 50 mu M DFO-B and 49 mu M Ox. The dissolution rates for FePO4 center dot 2H(2)O, alpha-FeOOH, and alpha-AlFeOOH correspond to 50, and 39-42 and 71-129 mu mol kg(-1) h(-1), respectively. The high extent of iron release from Al goethite is best explained because high-energy surface sites formed after Al substitution in goethite. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Cervini-Silva, Javiera] Univ Autonoma Metropolitana, Dept Proc & Tecnol, Div Ciencias Nat & Ingn, Unidad Cuajimalpa,UAM C, Delegacion Alvaro Obrego 01120, DF, Mexico.
[Cervini-Silva, Javiera; Banfield, Jillian] NASA, Astrobiol Inst, Washington, DC USA.
[Cervini-Silva, Javiera; Kearns, Josh; Banfield, Jillian] Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA USA.
[Banfield, Jillian] Univ Calif Berkeley, Ecosyst Sci Div, Berkeley, CA 94720 USA.
[Banfield, Jillian] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
RP Cervini-Silva, J (reprint author), Univ Autonoma Metropolitana, Dept Proc & Tecnol, Div Ciencias Nat & Ingn, Unidad Cuajimalpa,UAM C, Artificios 40,6 Piso, Delegacion Alvaro Obrego 01120, DF, Mexico.
EM jcervini@correo.cua.uam.mx
FU Mexican Academy of Sciences (Academia Mexicana de Ciencias); United
States-Mexico Foundation for Science (Fundacion Mexico-Estados Unidos
para la Ciencia) through the 2006-Young Researcher Summer Program
Fellowship (AMC-FUMEC); Universidad Autonoma Metropolitana Unidad
Cuajimalpa; NASA Astrobiology Institute [1-24190-31020-44]
FX JCS is most thankful to Lic. Maria del Rocio Galindo Ortega and Ms.
Maria Ines Escalante Vargas (UAM-Cuajimalpa) for their technical
assistance. JCS thanks the support of the Mexican Academy of Sciences
(Academia Mexicana de Ciencias) and The United States-Mexico Foundation
for Science (Fundacion Mexico-Estados Unidos para la Ciencia) through
the 2006-Young Researcher Summer Program Fellowship (AMC-FUMEC). This
project was supported in part by Universidad Autonoma Metropolitana
Unidad Cuajimalpa and the NASA Astrobiology Institute
(1-24190-31020-44).
NR 65
TC 6
Z9 6
U1 3
U2 36
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2541
J9 CHEM GEOL
JI Chem. Geol.
PD AUG 6
PY 2012
VL 320
BP 1
EP 8
DI 10.1016/j.chemgeo.2012.05.022
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 983OK
UT WOS:000307128400001
ER
PT J
AU Miller, MD
Adkins, JF
Menemenlis, D
Schodlok, MP
AF Miller, M. D.
Adkins, J. F.
Menemenlis, D.
Schodlok, M. P.
TI The role of ocean cooling in setting glacial southern source bottom
water salinity
SO PALEOCEANOGRAPHY
LA English
DT Article
ID OXYGEN ISOTOPIC COMPOSITION; ANTARCTIC ICE-SHEET; WEDDELL SEA;
DEEP-OCEAN; Z-COORDINATE; MODEL; TEMPERATURE; CIRCULATION; SHELF;
CLIMATE
AB At the Last Glacial Maximum (LGM), the salinity contrast between northern source deep water and southern source bottom water was reversed with respect to the contrast today. Additionally, Glacial Southern Source Bottom Water (GSSBW) was saltier than Antarctic Bottom Water (AABW), over and above the difference implied by the mean sea level change. This study examines to what extent cold temperatures, through their effect on ice formation and melting, could have caused these differences. Computational sensitivity experiments using a coupled ice shelf cavity-sea ice-ocean model are performed in a Weddell Sea domain, as a representative case study for bottom water formation originating from Antarctic continental shelves. Ocean temperatures at the domain open boundaries are systematically lowered to determine the sensitivity of Weddell Sea water mass properties to a range of cool ocean temperatures. The steady state salinities differ between experiments due to temperature-induced responses of ice shelf and sea ice melting and freezing, evaporation and open boundary fluxes. The results of the experiments indicate that reduced ocean temperature can explain up to 30% of the salinity difference between GSSBW and AABW, primarily due to decreased ice shelf melting. The smallest and most exposed ice shelves, which abut narrow continental shelves, have the greatest sensitivity to the ocean temperature changes, suggesting that at the LGM there could have been a shift in geographical site dominance in bottom water formation. More sea ice is formed and exported in the cold ocean experiments, but the effect of this on salinity is negated by an equal magnitude reduction in evaporation.
C1 [Miller, M. D.; Menemenlis, D.; Schodlok, M. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Schodlok, M. P.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Miller, MD (reprint author), CALTECH, Jet Prop Lab, MC 131-24,1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM madeline@caltech.edu
OI Miller, Madeline/0000-0003-2598-6518
FU National Science Foundation under NSF [OCE-0929272]; ECCO2 project; NASA
Advanced Supercomputing (NAS) Division
FX M.D.M. and J.F.A. received funding from the National Science Foundation
under NSF grant OCE-0929272. M.D.M., D.M., and M.P.S. received funding
from the ECCO2 project, a contribution to the NASA Modeling Analysis and
Prediction (MAP) Program. We gratefully acknowledge computational
resources and support from the NASA Advanced Supercomputing (NAS)
Division. We thank Keith Nicholls for providing the data for Figure 1.
Anand Gnanadesikan inspired writing the salt tracer code for analyzing
the sources of salinity changes. We are grateful to Martin Losch for his
implementation of the ice shelf code in MITgcm and for helpful
discussions about ice shelf and sea ice modeling.
NR 66
TC 9
Z9 9
U1 0
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0883-8305
J9 PALEOCEANOGRAPHY
JI Paleoceanography
PD AUG 4
PY 2012
VL 27
AR PA3207
DI 10.1029/2012PA002297
PG 16
WC Geosciences, Multidisciplinary; Oceanography; Paleontology
SC Geology; Oceanography; Paleontology
GA 984HY
UT WOS:000307181900001
ER
PT J
AU Chambers, FM
Booth, RK
De Vleeschouwer, F
Lamentowicz, M
Le Roux, G
Mauquoy, D
Nichols, JE
van Geel, B
AF Chambers, Frank M.
Booth, Robert K.
De Vleeschouwer, Francois
Lamentowicz, Mariusz
Le Roux, Gael
Mauquoy, Dmitri
Nichols, Jonathan E.
van Geel, Bas
TI Development and refinement of proxy-climate indicators from peats
SO QUATERNARY INTERNATIONAL
LA English
DT Article
ID TESTATE AMEBAS PROTOZOA; C-14 YR BP; N-ALKANE DISTRIBUTIONS; RAISED BOG
DEPOSITS; OMBROTROPHIC PEAT; LATE HOLOCENE; JURA MOUNTAINS; ATMOSPHERIC
PB; TRACE-ELEMENTS; PALEOENVIRONMENTAL RECONSTRUCTION
AB Peat, especially from acidic mires (bogs), is a natural archive of past environmental change. Reconstructions of past climate from bogs commenced in the 19th Century through examination of visible peat stratigraphy, and later formed the basis for a postglacial climatic scheme widely used in Northwest Europe. Nevertheless, misconceptions as to how bogs grow led to a 50-year lacuna in peat-climate study, before the concept of 'cyclic regeneration' in bogs was refuted. In recent decades, research using proxy-climate indicators from bogs has burgeoned. A range of proxies for past hydrological change has been developed, as well as use of pollen, bog oaks and pines and other data to reconstruct past temperatures. Most of this proxy-climate research has been carried out in Northern Europe, but peat-based research in parts of Asia and North America has increased, particularly during the last decade, while research has also been conducted in Australia, New Zealand and South America. This paper reviews developments in proxy-climate reconstructions from peatlands; chronicles use of a range of palaeo-proxies such as visible peat stratigraphy, plant macrofossils, peat humification, testate amoebae and non-pollen palynomorphs: and explains the use of wiggle-match radiocarbon dating and relationship to climate shifts. It details other techniques being used increasingly, such as biomarkers, stable-isotopes, inorganic geochemistry and estimation of dust flux: and points to new proxies under development. Although explicit protocols have been developed recently for research on ombrotrophic mires, it must be recognised that not all proxies and techniques have universal applicability, owing to differences in species assemblages, mire formation, topographic controls, and geochemical characteristics. (C) 2011 Elsevier Ltd and INQUA. All rights reserved.
C1 [Chambers, Frank M.] Univ Gloucestershire, Dept Nat & Social Sci, Ctr Environm Change & Quaternary Res, Cheltenham GL50 4AZ, Glos, England.
[Booth, Robert K.] Lehigh Univ, Dept Earth & Environm Sci, Bethlehem, PA 18015 USA.
[De Vleeschouwer, Francois] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Umea, Sweden.
[Lamentowicz, Mariusz] Adam Mickiewicz Univ, Fac Geog & Geol Sci, Dept Biogeog & Palaeoecol, PL-61680 Poznan, Poland.
[Le Roux, Gael] Univ Toulouse, EcoLab CNRS, F-31326 Castanet Tolosan, France.
[Mauquoy, Dmitri] Univ Aberdeen, Sch Geosci, Aberdeen AB24 3UF, Scotland.
[Nichols, Jonathan E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[van Geel, Bas] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, Dept Paleoecol & Landscape Ecol, NL-1098 XH Amsterdam, Netherlands.
RP Chambers, FM (reprint author), Univ Gloucestershire, Dept Nat & Social Sci, Ctr Environm Change & Quaternary Res, Francis Close Hall,Swindon Rd, Cheltenham GL50 4AZ, Glos, England.
EM fchambers@glos.ac.uk
RI Chambers, Frank/I-2965-2012; Le Roux, Gael/K-1154-2012; Lamentowicz,
Mariusz/E-8784-2010; Booth, Robert/G-5563-2010;
OI Chambers, Frank/0000-0002-0998-2093; Le Roux, Gael/0000-0002-1579-0178;
Lamentowicz, Mariusz/0000-0003-0429-1530; De Vleeschouwer,
Francois/0000-0002-0979-6397
FU US National Science Foundation; UK Quaternary Research Association
FX This paper arose from discussions at a Workshop, entitled Peatland
Archives of Holocene Climate Variability, held at Vihula Manor, Estonia,
May 2009, funded by the US National Science Foundation, the UK
Quaternary Research Association and facilitated by the University of
Tartu. A. Martinez-Cortizas, M. Kylander and W. Shotyk provided Pb
isotope data and allowed their use in Fig. 5.
NR 165
TC 48
Z9 53
U1 7
U2 90
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1040-6182
EI 1873-4553
J9 QUATERN INT
JI Quat. Int.
PD AUG 3
PY 2012
VL 268
BP 21
EP 33
DI 10.1016/j.quaint.2011.04.039
PG 13
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 990GH
UT WOS:000307618500003
ER
PT J
AU Li, FL
Jo, YH
Liu, WT
Yan, XH
AF Li, Feili
Jo, Young-Heon
Liu, W. Timothy
Yan, Xiao-Hai
TI A dipole pattern of the sea surface height anomaly in the North
Atlantic: 1990s-2000s
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID NONSTATIONARY TIME-SERIES; THERMOHALINE CIRCULATION; INTERANNUAL
VARIABILITY; SUBPOLAR GYRE; OCEAN; OSCILLATION; TRENDS; LEVEL
AB Despite a long-term trend of sea level rise continuing into the 2000s in the subpolar North Atlantic, variations in the sea surface height have behaved differently in both spatial and temporal domains. A dipole pattern, centered between the Northern Atlantic subpolar region and the region near the Gulf Stream, was observed in the linear trends of the sea surface height anomaly (SSHA). By applying the Ensemble Empirical Mode Decomposition (EEMD), we found that this dipole pattern is mainly associated with the interannual to decadal SSHA oscillations of the two regions, which are 180 degrees out of phase with each other over the time span of this study. The low-frequency variations of the SSHA in the subpolar region are strongly inversely correlated with the cumulative North Atlantic Oscillation (NAO) index (r = -0.84), in contrast with the Gulf Stream region, which is positively correlated (r = 0.22). This therefore reveals an asymmetric response of the regional SSHA to the cumulative NAO-forcing, in which the subpolar variability leads that of the Gulf Stream region by 29 months. Moreover, there is a remarkable reversal of the SSHA trends from the 1990s to the 2000s, which is unexpected given a weak and fluctuating NAO behavior since mid-1990s. Such SSHA variations in the 2000s might be related to the lagged variations of the Atlantic meridional overturning circulation (AMOC). Citation: Li, F., Y.-H. Jo, W. T. Liu, and X.-H. Yan (2012), A dipole pattern of the sea surface height anomaly in the North Atlantic: 1990s-2000s, Geophys. Res. Lett., 39, L15604, doi:10.1029/2012GL052556.
C1 [Li, Feili; Jo, Young-Heon; Yan, Xiao-Hai] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA.
[Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Yan, XH (reprint author), Univ Delaware, Coll Earth Ocean & Environm, 261 S Coll Ave, Newark, DE 19716 USA.
EM xiaohai@udel.edu
FU NASA Physical Oceanography Program; NASA EPSCoR Program; NASA Space
Grant; NOAA Sea Grant
FX The authors thank Federico Ienna for editorial assistance in English.
This research was partially supported by NASA Physical Oceanography
Program, NASA EPSCoR Program, NASA Space Grant, and NOAA Sea Grant. We
thank both anonymous reviewers for their insightful comments and
suggestions.
NR 27
TC 6
Z9 6
U1 1
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 3
PY 2012
VL 39
AR L15604
DI 10.1029/2012GL052556
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 988FN
UT WOS:000307474500005
ER
PT J
AU Fisher, JB
Badgley, G
Blyth, E
AF Fisher, Joshua B.
Badgley, Grayson
Blyth, Eleanor
TI Global nutrient limitation in terrestrial vegetation
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
ID NET PRIMARY PRODUCTIVITY; PLANT-SPECIES RICHNESS; WATER-ENERGY DYNAMICS;
LAND-USE TRANSITIONS; CARBON-CYCLE; NITROGEN DEPOSITION; CANOPY
NITROGEN; IMAGING SPECTROSCOPY; TROPICAL FORESTS; SECONDARY LANDS
AB Most vegetation is limited in productivity by nutrient availability, but the magnitude of limitation globally is not known. Nutrient limitation is directly relevant not only to ecology and agriculture, but also to the global carbon cycle by regulating how much atmospheric CO2 the terrestrial biosphere can sequester. We attempt to identify total nutrient limitation in terrestrial plant productivity globally using ecophysiological theory and new developments in remote sensing for evapotranspiration and plant productivity. Our map of nutrient limitation qualitatively reproduces known regional nutrient gradients (e.g., across Amazonia), highlights differences in nutrient addition to croplands (e.g., between "developed" and "developing" countries), identifies the role of nutrients on the distribution of major biomes (e.g., tree line migration in boreal North America), and compares similarly to a ground-based test along the Long Substrate Age Gradient in Hawaii, U.S.A. (e.g., foliar and soil nutrients, litter decomposition). Nonetheless, challenges in representing light and water use efficiencies, disturbance, and comparison to ground data with multiple interacting nutrients provide avenues for further progress on refining such a global map. Global average reduction in terrestrial plant productivity was within 16-28%, depending on treatment of disturbance; these values can be compared to global carbon cycle model estimates of carbon uptake reduction with nutrient cycle inclusion.
C1 [Fisher, Joshua B.; Badgley, Grayson] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Blyth, Eleanor] Ctr Ecol & Hydrol, Wallingford, Oxon, England.
RP Fisher, JB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM joshbfisher@gmail.com
RI Blyth, Eleanor/A-4010-2009;
OI Fisher, Joshua/0000-0003-4734-9085
FU National Aeronautics and Space Administration; Timothy S. Healy
Scholarship through Georgetown University; St. Cross College at Oxford
University; Oxford University's Environmental Change Institute
FX The research described in this paper was carried out by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Funding
for G.B. was provided by the Timothy S. Healy Scholarship through
Georgetown University and St. Cross College at Oxford University, as
well as by Oxford University's Environmental Change Institute. We thank
M. Zhao for providing the MOD15 product and C. Jimenez for providing ET
data. NASA/GEWEX SRB data were obtained from the NASA Langley Research
Center Atmospheric Sciences Data Center NASA/GEWEX SRB Project. J.-E.
Lee, C. Levitan, G. Miguez, A. Polhamus, M. Reichstein, and Y. Ryu
provided helpful comments.
NR 83
TC 30
Z9 31
U1 5
U2 115
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD AUG 3
PY 2012
VL 26
AR GB3007
DI 10.1029/2011GB004252
PG 9
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA 988FA
UT WOS:000307473000004
ER
PT J
AU Vaughan, DG
Corr, HFJ
Bindschadler, RA
Dutrieux, P
Gudmundsson, GH
Jenkins, A
Newman, T
Vornberger, P
Wingham, DJ
AF Vaughan, David G.
Corr, Hugh F. J.
Bindschadler, Robert A.
Dutrieux, Pierre
Gudmundsson, G. Hilmar
Jenkins, Adrian
Newman, Thomas
Vornberger, Patricia
Wingham, Duncan J.
TI Subglacial melt channels and fracture in the floating part of Pine
Island Glacier, Antarctica
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
ID ROSS ICE SHELF; BOTTOM CREVASSES; WEST ANTARCTICA; PENINSULA; BENEATH;
SHEET; DISINTEGRATION; MARGINS; FIELD
AB A dense grid of ice-penetrating radar sections acquired over Pine Island Glacier, West Antarctica has revealed a network of sinuous subglacial channels, typically 500 m to 3 km wide, and up to 200 m high, in the ice-shelf base. These subglacial channels develop while the ice is floating and result from melting at the base of the ice shelf. Above the apex of most channels, the radar shows isolated reflections from within the ice shelf. Comparison of the radar data with acoustic data obtained using an autonomous submersible, confirms that these echoes arise from open basal crevasses 50-100 m wide aligned with the subglacial channels and penetrating up to 1/3 of the ice thickness. Analogous sets of surface crevasses appear on the ridges between the basal channels. We suggest that both sets of crevasses were formed during the melting of the subglacial channels as a response to vertical flexing of the ice shelf toward the hydrostatic condition. Finite element modeling of stresses produced after the formation of idealized basal channels indicates that the stresses generated have the correct pattern and, if the channels were formed sufficiently rapidly, would have sufficient magnitude to explain the formation of the observed basal and surface crevasse sets. We conclude that ice-shelf basal melting plays a role in determining patterns of surface and basal crevassing. Increased delivery of warm ocean water into the sub-ice shelf cavity may therefore cause not only thinning but also structural weakening of the ice shelf, perhaps, as a prelude to eventual collapse.
C1 [Vaughan, David G.; Corr, Hugh F. J.; Dutrieux, Pierre; Gudmundsson, G. Hilmar; Jenkins, Adrian] British Antarctic Survey, Nat Environm Res Council, Cambridge CB3 0ET, England.
[Bindschadler, Robert A.] Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Newman, Thomas; Wingham, Duncan J.] UCL, Dept Earth Sci, CPOM, London, England.
[Vornberger, Patricia] Sci Applicat Int Corp, Beltsville, MD USA.
RP Vaughan, DG (reprint author), British Antarctic Survey, Nat Environm Res Council, Madingley Rd, Cambridge CB3 0ET, England.
EM d.vaughan@bas.ac.uk
RI Dutrieux, Pierre/B-7568-2012; Vaughan, David/C-8348-2011;
OI Dutrieux, Pierre/0000-0002-8066-934X; Gudmundsson, Gudmundur
Hilmar/0000-0003-4236-5369
FU Natural Environment Research Council; EU [226375]; NERC National Centre
for Earth Observation; NERC [NE/G001367/1]
FX We thank colleagues at British Antarctic Survey for constructive advice,
and in particular, Carl Robinson and Captain Doug Cochrane, who acquired
the radar data. The work is part of the British Antarctic Survey
program, Polar Science for Planet Earth funded in part by the Natural
Environment Research Council. DGV was funded by the EU FP7 program
ice2sea (grant 226375, pub. no. 076). TN and DJW acknowledge the support
of the NERC National Centre for Earth Observation. Autosub-3 data
collection and PD were supported by NERC Grant NE/G001367/1. Radar data
acquired for this study are available at
https://secure.antarctica.ac.uk/data/aerogeo/index.php
NR 56
TC 37
Z9 37
U1 2
U2 30
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 AUG 3
PY 2012
VL 117
AR F03012
DI 10.1029/2012JF002360
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA 988DD
UT WOS:000307467500002
ER
PT J
AU Mortin, J
Schroder, TM
Hansen, AW
Holt, B
McDonald, KC
AF Mortin, J.
Schroder, T. M.
Hansen, A. Walloe
Holt, B.
McDonald, K. C.
TI Mapping of seasonal freeze-thaw transitions across the pan-Arctic land
and sea ice domains with satellite radar
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID PASSIVE MICROWAVE RESPONSE; SNOW COVER; SCATTEROMETER DATA;
AMPLIFICATION; CO2; VARIABILITY; PARAMETERS; RADIOMETER; LATITUDES;
QUIKSCAT
AB To monitor the pan-Arctic seasonal freeze-thaw transitions of the land surface and sea ice, we analyze daily backscatter data from satellite scatterometry to examine the time series on an annual basis by applying an optimal edge detection scheme, and iterate against an internal median climatology to mitigate unreasonable outliers. By applying this novel algorithm to resolution-enhanced QuikSCAT data from 1999 to 2009, we have mapped a decade of seasonal freeze-thaw transitions across the landmass and sea ice north of 60 degrees N at a spatial resolution better than 5 km. The data set has been validated against surface air temperature measurements and snow depth obtained from a distributed network of weather stations and drift buoys. Most retrieved timings from surface and QuikSCAT measurements agree to less than a week at thaw transition for both land and sea ice and at freeze transition for sea ice, indicating successful retrieval over a range of surface covers. While the spatial pattern of freeze-thaw transition changes substantially from year to year, the interannual variability of the mean transition timing over a particular surface is small.
C1 [Mortin, J.] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden.
[Mortin, J.] Stockholm Univ, Bert Bolin Ctr Climate Res, S-10691 Stockholm, Sweden.
[Schroder, T. M.; Holt, B.; McDonald, K. C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Hansen, A. Walloe] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[McDonald, K. C.] CUNY City Coll, New York, NY 10031 USA.
RP Mortin, J (reprint author), Stockholm Univ, Dept Meteorol, Svante Arrhenius Vag 16C, S-10691 Stockholm, Sweden.
EM mortin@misu.su.se
FU NASA
FX The authors gratefully acknowledge the constructive remarks and valuable
input by Rune Grand Graversen and Gunilla Svensson at the Department of
Meteorology, Stockholm University, as well as by the two anonymous
reviewers. We thank Mark Ortmeyer at IABP for providing drift buoy data
and NCDC for providing terrestrial in situ data. Enhanced resolution
QuikSCAT data were obtained from the NASA sponsored Scatterometer
Climate Record Pathfinder at Brigham Young University through the
courtesy of David G. Long. This research was carried out at the
Department of Meteorology and the Bert Bolin Centre for Climate
Research, Stockholm University, as well as the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. This work was
supported under the NASA REASoN and MEaSUREs programs.
NR 67
TC 5
Z9 5
U1 2
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD AUG 3
PY 2012
VL 117
AR C08004
DI 10.1029/2012JC008001
PG 19
WC Oceanography
SC Oceanography
GA 988DJ
UT WOS:000307468100009
ER
PT J
AU Zhang, QH
Dunlop, MW
Lockwood, M
Lavraud, B
Bogdanova, YV
Hasegawa, H
Yang, HG
Liu, RY
Hu, HQ
Zhang, BC
Pu, ZY
Yang, ZW
Wang, J
Taylor, MGGT
Berchem, J
Constantinescu, D
Volwerk, M
Frey, H
Fazakerley, AN
Shen, C
Shi, JK
Sibeck, D
Escoubet, P
Wild, JA
AF Zhang, Q. -H.
Dunlop, M. W.
Lockwood, M.
Lavraud, B.
Bogdanova, Y. V.
Hasegawa, H.
Yang, H-G.
Liu, R. -Y.
Hu, H. -Q.
Zhang, B. -C.
Pu, Z. -Y.
Yang, Z. -W.
Wang, J.
Taylor, M. G. G. T.
Berchem, J.
Constantinescu, D.
Volwerk, M.
Frey, H.
Fazakerley, A. N.
Shen, C.
Shi, J. -K.
Sibeck, D.
Escoubet, P.
Wild, J. A.
TI Inner plasma structure of the low-latitude reconnection layer
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; FLUX-TRANSFER EVENTS; BOUNDARY-LAYER;
DAYSIDE MAGNETOPAUSE; NORTHWARD IMF; THEMIS; SIGNATURES; CLUSTER;
INSTRUMENT; DEPLETION
AB We report a clear transition through a reconnection layer at the low-latitude magnetopause which shows a complete traversal across all reconnected field lines during northwestward interplanetary magnetic field (IMF) conditions. The associated plasma populations confirm details of the electron and ion mixing and the time history and acceleration through the current layer. This case has low magnetic shear with a strong guide field and the reconnection layer contains a single density depletion layer on the magnetosheath side which we suggest results from nearly field-aligned magnetosheath flows. Within the reconnection boundary layer, there are two plasma boundaries, close to the inferred separatrices on the magnetosphere and magnetosheath sides (S-sp and S-sh) and two boundaries associated with the Alfven waves (or Rotational Discontinuities, RDsp and RDsh). The data are consistent with these being launched from the reconnection site and the plasma distributions are well ordered and suggestive of the time elapsed since reconnection of the field lines observed. In each sub-layer between the boundaries the plasma distribution is different and is centered around the current sheet, responsible for magnetosheath acceleration. We show evidence for a velocity dispersion effect in the electron anisotropy that is consistent with the time elapsed since reconnection. In addition, new evidence is presented for the occurrence of partial reflection of magnetosheath electrons at the magnetopause current layer.
C1 [Zhang, Q. -H.; Yang, H-G.; Liu, R. -Y.; Hu, H. -Q.; Zhang, B. -C.; Yang, Z. -W.] Polar Res Inst China, SOA Key Lab Polar Sci, Shanghai 200136, Peoples R China.
[Dunlop, M. W.; Lockwood, M.] Rutherford Appleton Lab, Chilton, England.
[Dunlop, M. W.; Shen, C.] Chinese Acad Sci, CSSAR, Beijing, Peoples R China.
[Lockwood, M.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Lavraud, B.] Inst Rech Astrophys & Planetol, Toulouse, France.
[Bogdanova, Y. V.; Fazakerley, A. N.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Hasegawa, H.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan.
[Pu, Z. -Y.; Wang, J.] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
[Taylor, M. G. G. T.; Escoubet, P.] ESA, ESTEC, Noordwijk, Netherlands.
[Berchem, J.] Univ Calif Los Angeles, IGPP, Los Angeles, CA USA.
[Constantinescu, D.] TU BS, Inst Geophys & Meteorol, Braunschweig, Germany.
[Volwerk, M.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Frey, H.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Sibeck, D.] NASA GSFC, Greenbelt, MD USA.
[Wild, J. A.] Univ Lancaster, Dept Phys, Lancaster, England.
RP Zhang, QH (reprint author), Polar Res Inst China, SOA Key Lab Polar Sci, 451 Jinqiao Rd, Shanghai 200136, Peoples R China.
EM zhangqinghe@pric.gov.cn
RI Hasegawa, Hiroshi/A-1192-2007; Sibeck, David/D-4424-2012; Lockwood,
Mike/G-1030-2011; Constantinescu, Dragos/A-6007-2013; Zhang,
Qing-He/G-4572-2014;
OI Frey, Harald/0000-0001-8955-3282; Wild, James/0000-0001-8025-8869;
Hasegawa, Hiroshi/0000-0002-1172-021X; Lockwood,
Mike/0000-0002-7397-2172; Zhang, Qing-He/0000-0003-2429-4050; Zhang,
Beichen/0000-0002-0927-9568
FU National Basic Research Program of China [2012CB825603]; National
Natural Science Foundation of China [41104091, 41031064, 40890164];
International Collaboration Supporting Project, Chinese Arctic and
Antarctic Administration [IC201112]; Ocean Public Welfare Scientific
Research Project, State Oceanic Administration People's Republic of
China [201005017]; Chinese Academy of Sciences (CAS) [2009S1-54]; NASA
[NAS5-02099]; German Ministry for Economy and Technology; German Center
for Aviation and Space (DLR) [50 OC 0302]
FX This work is supported by the National Basic Research Program of China
(grant 2012CB825603), the National Natural Science Foundation of China
(grants 41104091, 41031064, 40890164), the International Collaboration
Supporting Project, Chinese Arctic and Antarctic Administration
(IC201112), and Ocean Public Welfare Scientific Research Project, State
Oceanic Administration People's Republic of China (201005017). Part of
the work was done for the ISSI working group "Conjugate response of the
dayside magnetopause and dawn/dusk flanks using Cluster-THEMIS
conjunctions and ground based observations," which is led by M. W.
Dunlop and Y. V. Bogdanova. M. W. Dunlop is partly supported by Chinese
Academy of Sciences (CAS) visiting Professorship for senior
international scientists (grant 2009S1-54). We acknowledge NASA contract
NAS5-02099 and V. Angelopoulos for use of data from the THEMIS Mission.
Specifically: C. W. Carlson and J. P. McFadden for use of ESA data and
K. H. Glassmeier, U. Auster and W. Baumjohann for the use of FGM data
provided under the lead of the Technical University of Braunschweig and
with financial support through the German Ministry for Economy and
Technology and the German Center for Aviation and Space (DLR) under
contract 50 OC 0302.
NR 61
TC 5
Z9 7
U1 1
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD AUG 3
PY 2012
VL 117
AR A08205
DI 10.1029/2012JA017622
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 984HT
UT WOS:000307181400003
ER
PT J
AU Webb, N
Cseh, D
Lenc, E
Godet, O
Barret, D
Corbel, S
Farrell, S
Fender, R
Gehrels, N
Heywood, I
AF Webb, Natalie
Cseh, David
Lenc, Emil
Godet, Olivier
Barret, Didier
Corbel, Stephane
Farrell, Sean
Fender, Robert
Gehrels, Neil
Heywood, Ian
TI Radio Detections During Two State Transitions of the Intermediate-Mass
Black Hole HLX-1
SO SCIENCE
LA English
DT Article
ID X-RAY SOURCE; GALAXY ESO 243-49; FUNDAMENTAL PLANE; JETS; EMISSION;
OUTBURST; MODELS
AB Relativistic jets are streams of plasma moving at appreciable fractions of the speed of light. They have been observed from stellar-mass black holes (similar to 3 to 20 solar masses, M-circle dot) as well as supermassive black holes (similar to 10(6) to 10(9) M-circle dot) found in the centers of most galaxies. Jets should also be produced by intermediate-mass black holes (similar to 10(2) to 10(5) M-circle dot), although evidence for this third class of black hole has, until recently, been weak. We report the detection of transient radio emission at the location of the intermediate-mass black hole candidate ESO 243-49 HLX-1, which is consistent with a discrete jet ejection event. These observations also allow us to refine the mass estimate of the black hole to be between similar to 9 x 10(3) M-circle dot and similar to 9 x 10(4) M-circle dot.
C1 [Webb, Natalie; Godet, Olivier; Barret, Didier] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
[Webb, Natalie; Godet, Olivier; Barret, Didier] CNRS, IRAP, F-31028 Toulouse 4, France.
[Cseh, David; Corbel, Stephane] Univ Paris Diderot, Lab Astrophys Interact Multiechelles UMR 7158, CEA DSM CNRS, CEA Saclay, F-91191 Gif Sur Yvette, France.
[Lenc, Emil] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Lenc, Emil; Farrell, Sean] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia.
[Farrell, Sean] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Fender, Robert] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Gehrels, Neil] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Heywood, Ian] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
RP Webb, N (reprint author), Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
EM natalie.webb@irap.omp.eu
OI Lenc, Emil/0000-0002-9994-1593
FU European Community [ITN 215212]; UK Science and Technology Facilities
Council; Australian Research Council; Commonwealth of Australia;
[DP110102889]
FX Supported by the European Community's Seventh Framework Programme
(FP7/2007-2013) under grant agreement number ITN 215212 "Black Hole
Universe" (D. C. and S. C.), the UK Science and Technology Facilities
Council (S. F.), and an Australian Research Council postdoctoral
fellowship funded by grant DP110102889 (S. F.). The Australia Telescope
is funded by the Commonwealth of Australia for operation as a national
facility managed by CSIRO; the data can be accessed at
http://atoa.atnf.csiro.au/query.jsp. This work made use of data supplied
by the UK Swift Science Data Centre at the University of Leicester
(www.swift.ac.uk/swift_portal).
NR 28
TC 52
Z9 52
U1 0
U2 3
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 3
PY 2012
VL 337
IS 6094
BP 554
EP 556
DI 10.1126/science.1222779
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 982PU
UT WOS:000307058700037
PM 22767898
ER
PT J
AU Carter, JA
Agol, E
Chaplin, WJ
Basu, S
Bedding, TR
Buchhave, LA
Christensen-Dalsgaard, J
Deck, KM
Elsworth, Y
Fabrycky, DC
Ford, EB
Fortney, JJ
Hale, SJ
Handberg, R
Hekker, S
Holman, MJ
Huber, D
Karoff, C
Kawaler, SD
Kjeldsen, H
Lissauer, JJ
Lopez, ED
Lund, MN
Lundkvist, M
Metcalfe, TS
Miglio, A
Rogers, LA
Stello, D
Borucki, WJ
Bryson, S
Christiansen, JL
Cochran, WD
Geary, JC
Gilliland, RL
Haas, MR
Hall, J
Howard, AW
Jenkins, JM
Klaus, T
Koch, DG
Latham, DW
MacQueen, PJ
Sasselov, D
Steffen, JH
Twicken, JD
Winn, JN
AF Carter, Joshua A.
Agol, Eric
Chaplin, William J.
Basu, Sarbani
Bedding, Timothy R.
Buchhave, Lars A.
Christensen-Dalsgaard, Jorgen
Deck, Katherine M.
Elsworth, Yvonne
Fabrycky, Daniel C.
Ford, Eric B.
Fortney, Jonathan J.
Hale, Steven J.
Handberg, Rasmus
Hekker, Saskia
Holman, Matthew J.
Huber, Daniel
Karoff, Christopher
Kawaler, Steven D.
Kjeldsen, Hans
Lissauer, Jack J.
Lopez, Eric D.
Lund, Mikkel N.
Lundkvist, Mia
Metcalfe, Travis S.
Miglio, Andrea
Rogers, Leslie A.
Stello, Dennis
Borucki, William J.
Bryson, Steve
Christiansen, Jessie L.
Cochran, William D.
Geary, John C.
Gilliland, Ronald L.
Haas, Michael R.
Hall, Jennifer
Howard, Andrew W.
Jenkins, Jon M.
Klaus, Todd
Koch, David G.
Latham, David W.
MacQueen, Phillip J.
Sasselov, Dimitar
Steffen, Jason H.
Twicken, Joseph D.
Winn, Joshua N.
TI Kepler-36: A Pair of Planets with Neighboring Orbits and Dissimilar
Densities
SO SCIENCE
LA English
DT Article
ID TRANSIT TIMING VARIATIONS; LOW-MASS; STAR; MISSION; SYSTEMS;
PERFORMANCE; STABILITY; COMPANION; SCIENCE; CURVES
AB In the solar system, the planets' compositions vary with orbital distance, with rocky planets in close orbits and lower-density gas giants in wider orbits. The detection of close-in giant planets around other stars was the first clue that this pattern is not universal and that planets' orbits can change substantially after their formation. Here, we report another violation of the orbit-composition pattern: two planets orbiting the same star with orbital distances differing by only 10% and densities differing by a factor of 8. One planet is likely a rocky "super-Earth," whereas the other is more akin to Neptune. These planets are 20 times more closely spaced and have a larger density contrast than any adjacent pair of planets in the solar system.
C1 [Carter, Joshua A.; Holman, Matthew J.; Geary, John C.; Latham, David W.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Chaplin, William J.; Elsworth, Yvonne; Hale, Steven J.; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Edgbaston B15 2TT, England.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Bedding, Timothy R.; Stello, Dennis] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
[Christensen-Dalsgaard, Jorgen; Handberg, Rasmus; Karoff, Christopher; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Deck, Katherine M.; Rogers, Leslie A.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Deck, Katherine M.; Rogers, Leslie A.; Winn, Joshua N.] Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Fabrycky, Daniel C.; Fortney, Jonathan J.; Lopez, Eric D.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, Netherlands Sch Phys, Amsterdam, Netherlands.
[Christiansen, Jessie L.; Jenkins, Jon M.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA.
[Cochran, William D.; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Hall, Jennifer; Klaus, Todd] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Howard, Andrew W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
RP Carter, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jacarter@cfa.harvard.edu; agol@astro.washington.edu
RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Agol,
Eric/B-8775-2013; Basu, Sarbani/B-8015-2014; Hale, Steven/E-3472-2015;
OI Buchhave, Lars A./0000-0003-1605-5666; Bedding,
Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416;
Bedding, Tim/0000-0001-5222-4661; Kawaler, Steven/0000-0002-6536-6367;
Agol, Eric/0000-0002-0802-9145; Basu, Sarbani/0000-0002-6163-3472; Hale,
Steven/0000-0002-6402-8382; Fortney, Jonathan/0000-0002-9843-4354;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [HF-51267.01-A, HF-51272.01-A,
NAS 5-26555]; Space Telescope Science Institute; NSF [AST-0645416];
Center for Astrophysics; UK Science and Technology Facilities Council
(STFC); Danish National Research Foundation; ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler); European Research
Council [267864]; Netherlands Organization for Scientific Research
(NWO); NASA Kepler Participating Scientist program [NNX12AC76G]
FX NASA's Science Mission Directorate provided funding for the Kepler
Discovery mission. J.A.C. and D. C. F. acknowledge support by NASA
through Hubble Fellowship grants HF-51267.01-A and HF-51272.01-A awarded
by the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Incorporated, for
NASA, under contract NAS 5-26555. E. A. acknowledges NSF Career grant
AST-0645416 and thanks the Center for Astrophysics, where this work
began. W.J.C., A. M., and Y.E. acknowledge the financial support of the
UK Science and Technology Facilities Council (STFC). Funding for the
Stellar Astrophysics Centre (SAC) is provided by the Danish National
Research Foundation. The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (grant agreement no. 267864). S. H.
acknowledges financial support from the Netherlands Organization for
Scientific Research (NWO). Computational time on Kraken at the National
Institute of Computational Sciences was provided through NSF TeraGrid
allocation TG-AST090107. J.N.W. was supported by the NASA Kepler
Participating Scientist program through grant NNX12AC76G. Refer to the
supplementary materials for access information to data used in this
work.
NR 26
TC 148
Z9 149
U1 8
U2 18
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 3
PY 2012
VL 337
IS 6094
BP 556
EP 559
DI 10.1126/science.1223269
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 982PU
UT WOS:000307058700038
PM 22722249
ER
PT J
AU Yu, HB
Remer, LA
Chin, M
Bian, HS
Tan, Q
Yuan, TL
Zhang, Y
AF Yu, Hongbin
Remer, Lorraine A.
Chin, Mian
Bian, Huisheng
Tan, Qian
Yuan, Tianle
Zhang, Yan
TI Aerosols from Overseas Rival Domestic Emissions over North America
SO SCIENCE
LA English
DT Article
ID BLACK CARBON; DUST; TRANSPORT; POLLUTION; AERONET; CALIPSO; MODEL
AB Many types of aerosols have lifetimes long enough for their transcontinental transport, making them potentially important contributors to air quality and climate change in remote locations. We estimate that the mass of aerosols arriving at North American shores from overseas is comparable with the total mass of particulates emitted domestically. Curbing domestic emissions of particulates and precursor gases, therefore, is not sufficient to mitigate aerosol impacts in North America. The imported contribution is dominated by dust leaving Asia, not by combustion-generated particles. Thus, even a reduction of industrial emissions of the emerging economies of Asia could be overwhelmed by an increase of dust emissions due to changes in meteorological conditions and potential desertification.
C1 [Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Yu, Hongbin; Chin, Mian; Bian, Huisheng; Tan, Qian; Yuan, Tianle; Zhang, Yan] NASA, Earth Sci Directorate, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Remer, Lorraine A.; Bian, Huisheng; Yuan, Tianle] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Tan, Qian; Zhang, Yan] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Ctr, Columbia, MD 21044 USA.
RP Yu, HB (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
EM hongbin.yu@nasa.gov
RI Yu, Hongbin/C-6485-2008; Chin, Mian/J-8354-2012; Yuan,
Tianle/D-3323-2011; Zhang, Yan/C-4792-2012
OI Yu, Hongbin/0000-0003-4706-1575;
FU NASA [NNXAH66G, NNX11AJ91G]; GMI [NNX10AK61G]
FX We acknowledge the NASA support of this work via NNXAH66G (The Science
of Terra and Aqua Program) and NNX11AJ91G (Atmospheric Composition
Modeling and Analysis Program) (H.Y.), both managed by R. Eckman. The
NASA Modeling, Analysis, and Prediction program managed by D. Considine
is acknowledged for supporting the model development of GOCART (M. C.)
and GMI (H. B., under NNX10AK61G). We are grateful to J. Zhang for
providing his reprocessed MODIS data, Z. Liu for providing insights in
the lidar characterization of Asian dust, and X. Pan for acquiring
CALIOP data. The MODIS data were obtained from the NASA Level 1 and
Atmosphere Archive and Distribution System. The CALIOP data were
obtained from the NASA Langley Research Center Atmospheric Science Data
Center.
NR 27
TC 85
Z9 87
U1 7
U2 66
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 3
PY 2012
VL 337
IS 6094
BP 566
EP 569
DI 10.1126/science.1217576
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 982PU
UT WOS:000307058700041
PM 22859485
ER
PT J
AU Suh, M
Meyyappan, M
Ju, S
AF Suh, Misook
Meyyappan, M.
Ju, Sanghyun
TI The effect of Ga content on In2xGa2-2xO3 nanowire transistor
characteristics
SO NANOTECHNOLOGY
LA English
DT Article
ID DOPED INDIUM OXIDE; CHEMICAL-VAPOR-DEPOSITION; IN2O3 NANOWIRES;
OPTICAL-PROPERTIES; THIN-FILMS; GROWTH; ARRAYS; GA2O3
AB We have investigated the change in structural and electrical properties of In2xGa2-2xO3 nanowires (x = 1, 0.69 and 0.32) grown with varied indium (In) and gallium (Ga) contents. The as-grown In2xGa2-2xO3 nanowires kept the cubic crystal structure of In2O3 intact even when the atomic percentages of Ga were increased to 31% (x = 0.69) and 68% (x = 0.32) in comparison to the total amount of In and Ga. However, as Ga added to In2O3 structure was substituted with In, the lattice constant decreased and, consequently, the main peaks observed in x-ray diffraction in the direction of (222), (400) and (440) shifted by around similar to 0.08 degrees. The average threshold voltage values for the In2xGa2-2xO3 nanowire transistors were -9.9 V (x = 1), -6.6 V (x = 0.67) and -5.6 V (x = 0.32), exhibiting a more positive shift and the sub-threshold slope increased to 0.53 V/dec (x = 1), 0.33 V/dec (x = 0.67) and 0.27 V/dec (x = 0.32), showing an improved switching characteristic with increasing Ga.
C1 [Suh, Misook; Ju, Sanghyun] Kyonggi Univ, Dept Phys, Suwon 443760, Gyeonggi Do, South Korea.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Meyyappan, M.] POSTECH, Div IT Convergence Engn, Pohang, South Korea.
RP Suh, M (reprint author), Kyonggi Univ, Dept Phys, Suwon 443760, Gyeonggi Do, South Korea.
EM shju@kgu.ac.kr
FU National Research Foundation of Korea (NRF); Ministry of Education,
Science and Technology [2011-0023219, 2011-0019133, 2011K000627];
Ministry of Education, Science and Technology through the National
Research Foundation of Korea [R31-10100]
FX This research was supported by the National Research Foundation of Korea
(NRF) funded by the Ministry of Education, Science and Technology
(2011-0023219, 2011-0019133 and 2011K000627). The World Class University
program at POSTECH funded by the Ministry of Education, Science and
Technology through the National Research Foundation of Korea (R31-10100)
is also acknowledged.
NR 26
TC 7
Z9 7
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD AUG 3
PY 2012
VL 23
IS 30
AR 305203
DI 10.1088/0957-4484/23/30/305203
PG 5
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 973DF
UT WOS:000306333500004
PM 22750916
ER
PT J
AU Zhi, MJ
Koneru, A
Yang, F
Manivannan, A
Li, J
Wu, NQ
AF Zhi, Mingjia
Koneru, Anveeksh
Yang, Feng
Manivannan, Ayyakkannu
Li, Jing
Wu, Nianqiang
TI Electrospun La0.8Sr0.2MnO3 nanofibers for a high-temperature
electrochemical carbon monoxide sensor
SO NANOTECHNOLOGY
LA English
DT Article
ID GAS SENSORS; SENSING ELECTRODE; FUEL-CELL; CO; CATHODE
AB Lanthanum strontium manganite (La0.8Sr0.2MnO3, LSM) nanofibers have been synthesized by the electrospinning method. The electrospun nanofibers are intact without morphological and structural changes after annealing at 1050 degrees C. The LSM nanofibers are employed as the sensing electrode of an electrochemical sensor with yttria-stabilized zirconia (YSZ) electrolyte for carbon monoxide detection at high temperatures over 500 degrees C. The electrospun nanofibers form a porous network electrode, which provides a continuous pathway for charge transport. In addition, the nanofibers possess a higher specific surface area than conventional micron-sized powders. As a result, the nanofiber electrode exhibits a higher electromotive force and better electro-catalytic activity toward CO oxidation. Therefore, the sensor with the nanofiber electrode shows a higher sensitivity, lower limit of detection and faster response to CO than a sensor with a powder electrode.
C1 [Zhi, Mingjia; Koneru, Anveeksh; Wu, Nianqiang] W Virginia Univ, Dept Mech & Aerosp Engn, Morgantown, WV 26506 USA.
[Yang, Feng] W Virginia Univ, Ind & Management Syst Engn Dept, Morgantown, WV 26506 USA.
[Manivannan, Ayyakkannu] US DOE, Natl Energy Technol Lab, Morgantown, WV 26507 USA.
[Li, Jing] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Zhi, MJ (reprint author), W Virginia Univ, Dept Mech & Aerosp Engn, Morgantown, WV 26506 USA.
EM nick.wu@mail.wvu.edu
RI Zhi, Mingjia/A-6866-2010; Wu, Nianqiang/B-9798-2015
OI Zhi, Mingjia/0000-0002-4291-0809; Wu, Nianqiang/0000-0002-8888-2444
FU NASA WV; NASA West Virginia EPSCoR; Research Challenge Grant from the
State of West Virginia [EPS08-01]; NSF [EPS 1003907]; West Virginia
University Research Corporation
FX The work was partially supported by NASA WV Space Grant Program and NASA
West Virginia EPSCoR. The resource and facilities used in this work were
partially sponsored by a Research Challenge Grant from the State of West
Virginia (EPS08-01), an NSF (EPS 1003907) grant, and the West Virginia
University Research Corporation.
NR 28
TC 10
Z9 10
U1 6
U2 67
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD AUG 3
PY 2012
VL 23
IS 30
AR 305501
DI 10.1088/0957-4484/23/30/305501
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 973DF
UT WOS:000306333500017
PM 22751138
ER
PT J
AU Yu, JY
Zou, YH
Kim, ST
Lee, T
AF Yu, Jin-Yi
Zou, Yuhao
Kim, Seon Tae
Lee, Tong
TI The changing impact of El Nino on US winter temperatures
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ENSO TELECONNECTIONS; HEMISPHERE WINTER; PRECIPITATION; ANOMALIES;
PACIFIC; EVOLUTION; EVENTS
AB In this study, evidence is presented from statistical analyses, numerical model experiments, and case studies to show that the impact on US winter temperatures is different for the different types of El Nino. While the conventional Eastern-Pacific El Nino affects winter temperatures primarily over the Great Lakes, Northeast, and Southwest US, the largest impact from Central-Pacific El Nino is on temperatures in the northwestern and southeastern US. The recent shift to a greater frequency of occurrence of the Central-Pacific type has made the Northwest and Southeast regions of the US most influenced by El Nino. It is shown that the different impacts result from differing wave train responses in the atmosphere to the sea surface temperature anomalies associated with the two types of El Nino. Citation: Yu, J.-Y., Y. Zou, S. T. Kim, and T. Lee (2012), The changing impact of El Nino on US winter temperatures, Geophys. Res. Lett., 39, L15702, doi:10.1029/2012GL052483.
C1 [Yu, Jin-Yi; Zou, Yuhao; Kim, Seon Tae] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Yu, JY (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM jyyu@uci.edu
RI Kim, Seon Tae/G-6361-2011; Yu, Jin-Yi/G-3413-2011
OI Kim, Seon Tae/0000-0003-2628-0904; Yu, Jin-Yi/0000-0001-6156-7623
FU NOAAMAPP grant [NA11OAR4310102]; NSF grant [ATM-0925396]
FX We thank two anonymous reviewers and the Editor Noah Diffenbaugh for
their valuable comments. This research was supported by NOAAMAPP grant
NA11OAR4310102 and NSF grant ATM-0925396.
NR 23
TC 68
Z9 69
U1 3
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 AUG 2
PY 2012
VL 39
AR L15702
DI 10.1029/2012GL052483
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 988FK
UT WOS:000307474200003
ER
PT J
AU Carley, RA
Whaler, KA
Purucker, ME
Halekas, JS
AF Carley, R. A.
Whaler, K. A.
Purucker, M. E.
Halekas, J. S.
TI Magnetization of the lunar crust
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID BASIN-FORMING IMPACTS; REMANENT MAGNETIZATION; DYNAMO DRIVEN; CORE
DYNAMO; FIELD; MAGNETISM; MOON; PROSPECTOR; ANOMALIES; MAGNETOMETER
AB Magnetic fields measured by the satellite Lunar Prospector show large scale features resulting from remanently magnetized crust. Vector data synthesized at satellite altitude from a spherical harmonic model of the lunar crustal field, and the radial component of the magnetometer data, have been used to produce spatially continuous global magnetization models for the lunar crust. The magnetization is expressed in terms of localized basis functions, with a magnetization solution selected having the smallest root-mean square magnetization for a given fit to the data, controlled by a damping parameter. Suites of magnetization models for layers with thicknesses between 10 and 50 km are able to reproduce much of the input data, with global misfits of less than 0.5 nT (within the uncertainties of the data), and some surface field estimates. The magnetization distributions show robust magnitudes for a range of model thicknesses and damping parameters, however the magnetization direction is unconstrained. These global models suggest that magnetized sources of the lunar crust can be represented by a 30 km thick magnetized layer. Average magnetization values in magnetized regions are 30-40 mA/m, similar to the measured magnetizations of the Apollo samples and significantly weaker than crustal magnetizations for Mars and the Earth. These are the first global magnetization models for the Moon, providing lower bounds on the magnitude of lunar crustal magnetization in the absence of multiple sample returns, and can be used to predict the crustal contribution to the lunar magnetic field at a particular location.
C1 [Carley, R. A.; Whaler, K. A.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JW, Midlothian, Scotland.
[Purucker, M. E.] NASA, Goddard Space Flight Ctr, SGT, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Halekas, J. S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Carley, RA (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JW, Midlothian, Scotland.
EM r.a.carley@cantab.net
OI Halekas, Jasper/0000-0001-5258-6128
FU Natural Environment Research Council [NER/S/A/2006/14230]
FX This research was funded by the Natural Environment Research Council
(NER/S/A/2006/14230). Maps are plotted using Generic Mapping Tools
[Wessel and Smith, 1998]. We would like to thank Benoit Langlais, Mark
Wieczorek and two anonymous reviewers for their helpful and insightful
suggestions.
NR 57
TC 3
Z9 4
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD AUG 2
PY 2012
VL 117
AR E08001
DI 10.1029/2011JE003944
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 988EJ
UT WOS:000307471000001
ER
PT J
AU Baker, DN
AF Baker, Daniel N.
TI Let academia lead space science
SO NATURE
LA English
DT Editorial Material
C1 [Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Baker, Daniel N.] NASAs Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD USA.
RP Baker, DN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM daniel.baker@lasp.colorado.edu
NR 0
TC 0
Z9 0
U1 0
U2 2
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD AUG 2
PY 2012
VL 488
IS 7409
BP 27
EP 28
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 981ZE
UT WOS:000307010700016
PM 22859186
ER
PT J
AU Dismukes, RK
AF Dismukes, R. Key
TI Prospective Memory in Workplace and Everyday Situations
SO CURRENT DIRECTIONS IN PSYCHOLOGICAL SCIENCE
LA English
DT Article
DE prospective memory; intentions; paradigms; workplace; countermeasures
ID RETRIEVAL-PROCESSES; INTENSIVE-CARE; INTENTIONS; AGE; INTERRUPTIONS;
EVENTS; COST
AB Forgetting to perform intended actions can have major consequences, including loss of life in some situations. Laboratory research on prospective memory-remembering (and sometimes forgetting) to perform deferred intentions-is growing rapidly, thanks to new laboratory paradigms that are being used to uncover underlying cognitive mechanisms. Everyday situations and workplace situations in fields such as aviation and medicine, which have been studied less extensively, reveal aspects of prospective remembering that have both practical and theoretical implications, which are discussed here. Several types of situations in which individuals are vulnerable to forgetting intentions, but which have not been studied extensively in laboratory research, are described, and ways to reduce vulnerability to forgetting are suggested.
C1 [Dismukes, R. Key] NASA, Ames Res Ctr, Washington, DC 20546 USA.
RP Dismukes, RK (reprint author), 167 River Rock Dr, Dahlonega, GA 30533 USA.
EM rkeydismukes@gmail.com
NR 36
TC 24
Z9 24
U1 0
U2 19
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0963-7214
J9 CURR DIR PSYCHOL SCI
JI Curr. Dir. Psychol.
PD AUG
PY 2012
VL 21
IS 4
BP 215
EP 220
DI 10.1177/0963721412447621
PG 6
WC Psychology, Multidisciplinary
SC Psychology
GA 083LD
UT WOS:000314464300001
ER
PT J
AU David, C
Haefele, A
Keckhut, P
Marchand, M
Jumelet, J
Leblanc, T
Cenac, C
Laqui, C
Porteneuve, J
Haeffelin, M
Courcoux, Y
Snels, M
Viterbini, M
Quatrevalet, M
AF David, C.
Haefele, A.
Keckhut, P.
Marchand, M.
Jumelet, J.
Leblanc, T.
Cenac, C.
Laqui, C.
Porteneuve, J.
Haeffelin, M.
Courcoux, Y.
Snels, M.
Viterbini, M.
Quatrevalet, M.
TI Evaluation of stratospheric ozone, temperature, and aerosol profiles
from the LOANA lidar in Antarctica
SO POLAR SCIENCE
LA English
DT Article
DE Polar ozone; Polar stratospheric clouds; Lidar; Stratosphere
ID DUMONT DURVILLE ANTARCTICA; CIRRUS CLOUDS; VOLCANIC AEROSOLS;
EXTINCTION; ATMOSPHERE; SYSTEM
AB We present an evaluation of observations from the Lidar Ozone and Aerosol for NDACC in Antarctica (LOANA) at the Dumont d'Urville station, Antarctica. This instrument is part of the Network for the Detection of Atmospheric Composition Change (NDACC), and ensures continuity with lidar measurements made since 1989 with the previous instrument at this site. This study is based on the dataset from 2008 to 2009, and comparisons are made with observations from balloon soundings, and from three satellite experiments: Aura/MLS, TIMED/SABER, and CALIOP/CALIPSO. The lidar ozone data are in very good agreement with the balloon sounding data (ECC sensor), revealing a bias of less than 3% between 17 and 34 km. For temperature, the lidar shows a low bias of -3 K at 20 km when compared with Aura/MLS. Between 30 and 50 km, the bias is less than 2 K. We also present our initial results showing diurnal variations in temperature. The amplitude of these diurnal cycles is on the order of 1 K and is unlikely to account for the temperature biases between LOANA and the reference instruments. Comparisons of total attenuated backscatter reveal good qualitative agreement between LOANA and CALIOP, with differences of less than 30% in the derived optical depth. (c) 2012 Elsevier B.V. and NIPR. All rights reserved.
C1 [David, C.; Haefele, A.; Keckhut, P.; Marchand, M.; Jumelet, J.; Cenac, C.; Laqui, C.; Porteneuve, J.] Univ Versailles St Quentin, LATMOS IPSL, F-78280 Guyancourt, France.
[Leblanc, T.] CALTECH, Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA.
[Cenac, C.; Haeffelin, M.] Ecole Polytech, Lab Meteorol Dynam IPSL, F-91128 Palaiseau, France.
[Courcoux, Y.] CNRS, Observ Phys Atmosphere La Reunion, F-97715 St Denis, France.
[Snels, M.; Viterbini, M.] ISAC CNR, I-00133 Rome, Italy.
[David, C.] Inst Polaire Francais Paul Emile Victor, F-29280 Plouzane, France.
[Haefele, A.] MeteoSwiss, CH-1530 Payerne, Switzerland.
[Quatrevalet, M.] Deutsch Zentrum Luft & Raumfahrt, Inst Phys & Atmosphare, Oberpfaffenhofen, Germany.
RP Haefele, A (reprint author), MeteoSwiss, Chemin Aerol, CH-1530 Payerne, Switzerland.
EM alexander.haefele@meteoswiss.ch
RI Snels, Marcel/J-2324-2012
OI Snels, Marcel/0000-0002-3025-5237
NR 31
TC 2
Z9 2
U1 4
U2 17
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1873-9652
J9 POLAR SCI
JI Polar Sci.
PD AUG-NOV
PY 2012
VL 6
IS 3-4
BP 209
EP 225
DI 10.1016/j.polar.2012.07.001
PG 17
WC Ecology; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 094BM
UT WOS:000315238000001
ER
PT J
AU Derkowski, A
Bristow, TF
AF Derkowski, Arkadiusz
Bristow, Thomas F.
TI ON THE PROBLEMS OF TOTAL SPECIFIC SURFACE AREA AND CATION EXCHANGE
CAPACITY MEASUREMENTS IN ORGANIC-RICH SEDIMENTARY ROCKS
SO CLAYS AND CLAY MINERALS
LA English
DT Article
DE Bitumen; CEC; EGME; Kerogen; Organic Matter; Shale; Specific Surface
Area
ID LAYER CHARGE; CARBON ISOTOPES; EGME RETENTION; BLACK SHALE; KEROGEN;
SMECTITE; SORPTION; MATTER; SOILS; CLAY
AB The increasing exploration and exploitation of hydrocarbon resources hosted by oil and gas shales demands the correct measurement of certain properties of sedimentary rocks rich in organic matter (OM). Two essential properties of OM-rich shales, the total specific surface area (TSSA) and cation exchange capacity (CEC), are primarily controlled by the rock's clay mineral content (i.e. the type and quantity). This paper presents the limitations of two commonly used methods of measuring bulk-rock TSSA and CEC, ethylene glycol monoethyl ether (EGME) retention and visible light spectrometry of Co(III)-hexamine, in OM-rich rocks. The limitations were investigated using a suite of OM-rich shales and mudstones that vary in origin, age, clay mineral content, and thermal maturity.
Ethylene glycol monoethyl ether reacted strongly with and was retained by natural OM, producing excess TSSA if calculated using commonly applied adsorption coefficients. Although the intensity of the reaction seems to depend on thermal maturity, OM in all the samples analyzed reacted with EGME to an extent that made TSSA values unreliable; therefore, EGME is not recommended for TSSA measurements on samples containing >3% OM.
Some evidence indicated that drying at >= 200 degrees C may influence bulk-rock CEC values by altering OM in early mature rocks. In light of this evidence, drying at 110 C is recommended as a more suitable pretreatment for CEC measurements in OM-rich shales. When using visible light spectrometry for CEC determination, leachable sample components contributed to the absorbance of the measured wavelength (470 nm), decreasing the calculated bulk rock CEC value. A test of sample-derived excess absorbance with zero-absorbance solutions (i.e. NaCl) and the introduction of corrections to the CEC calculation are recommended.
C1 [Derkowski, Arkadiusz] Polish Acad Sci, INGPAN, Inst Geol Sci, PL-31002 Krakow, Poland.
[Bristow, Thomas F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Derkowski, A (reprint author), Polish Acad Sci, INGPAN, Inst Geol Sci, Senacka 1, PL-31002 Krakow, Poland.
EM ndderkow@cyf-kr.edu.pl
NR 62
TC 10
Z9 11
U1 2
U2 31
PU CLAY MINERALS SOC
PI CHANTILLY
PA 3635 CONCORDE PKWY, STE 500, CHANTILLY, VA 20151-1125 USA
SN 0009-8604
J9 CLAY CLAY MINER
JI Clay Clay Min.
PD AUG
PY 2012
VL 60
IS 4
BP 348
EP 362
DI 10.1346/CCMN.2012.0600402
PG 15
WC Chemistry, Physical; Geosciences, Multidisciplinary; Mineralogy; Soil
Science
SC Chemistry; Geology; Mineralogy; Agriculture
GA 035TP
UT WOS:000310972300002
ER
PT J
AU Stierhoff, KL
Neuman, M
Butler, JL
AF Stierhoff, Kevin L.
Neuman, Melissa
Butler, John L.
TI On the road to extinction? Population declines of the endangered white
abalone, Haliotis sorenseni
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE Visual transect survey; Remotely operated vehicle; Endangered species;
Allee effect
ID SOUTHERN-CALIFORNIA; CRACHERODII LEACH; RECRUITMENT; GASTROPODA;
MOLLUSCA; BIOLOGY; GROWTH
AB In 2001, the white abalone (Haliotis sorenseni) became the first marine invertebrate to be listed as endangered under the Endangered Species Act (ESA). Low densities and recruitment failure due to Allee effects were identified as being the major threats to the species' long-term viability. Visual transect surveys conducted using a remotely operated vehicle (ROV) since 2002 indicate a dramatic and continued decline in white abalone total abundance (similar to 78% decrease) and density (33-100% decrease, depending on depth and year) between 2002 and 2010 at Tanner Bank, an area of historically high abundance (>1/m(2)). An increase in the size distribution over this same time period suggests individuals in the white abalone population are growing larger (and aging) with little or no indication of adequate recruitment success. The vast majority (between 77% and 89%, depending on the year) of white abalone were observed alone, which suggests that the likelihood of reproductive success within this population remains very low. The continuing decline 30 years after the last major commercial harvest demonstrates that the strategy of benign neglect, or allowing the population to recover without intervention, has clearly failed. We recommend immediate proactive conservation through population enhancement by out-planting healthy, captive-bred white abalone in areas where populations have reached or are approaching local extinction. Published by Elsevier Ltd.
C1 [Stierhoff, Kevin L.; Butler, John L.] NOAA, Fisheries Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA.
[Neuman, Melissa] NOAA, Protected Resources Div, SW Reg Off, Natl Marine Fisheries Serv, Long Beach, CA 90802 USA.
RP Stierhoff, KL (reprint author), NOAA, Fisheries Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 8604 La Jolla Shores Dr, La Jolla, CA 92037 USA.
EM kevin.stierhoff@noaa.gov
RI Stierhoff, Kevin/A-7624-2013
OI Stierhoff, Kevin/0000-0002-3058-0312
NR 40
TC 14
Z9 14
U1 6
U2 48
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
J9 BIOL CONSERV
JI Biol. Conserv.
PD AUG
PY 2012
VL 152
BP 46
EP 52
DI 10.1016/j.biocon.2012.03.013
PG 7
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 983AI
UT WOS:000307088200006
ER
PT J
AU Krause, DE
Rogers, BA
Fischbach, E
Buncher, JB
Ging, A
Jenkins, JH
Longuski, JM
Strange, N
Sturrock, PA
AF Krause, D. E.
Rogers, B. A.
Fischbach, E.
Buncher, J. B.
Ging, A.
Jenkins, J. H.
Longuski, J. M.
Strange, N.
Sturrock, P. A.
TI Searches for solar-influenced radioactive decay anomalies using
spacecraft RTGs
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Radioactive decay; Sun; Deep-space probes; New forces; Neutrinos
ID LONG-RANGE FORCES; HALF-LIFE; BETA-DECAY; NEUTRINO; RATES; MASS
AB Experiments showing a seasonal variation of the nuclear decay rates of a number of different nuclei, and decay anomalies apparently related to solar flares and solar rotation, have suggested that the Sun may somehow be influencing nuclear decay processes. Recently. Cooper searched for such an effect in Pu-238 nuclei contained in the radioisotope thermoelectric generators (RTGs) on board the Cassini spacecraft. In this paper we modify and extend Cooper's analysis to obtain constraints on anomalous decays of Pu-238 over a wider range of models, but these limits cannot be applied to other nuclei if the anomaly is composition-dependent. We also show that it may require very high sensitivity for terrestrial experiments to discriminate among some models if such a decay anomaly exists, motivating the consideration of future spacecraft experiments which would require less precision. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Krause, D. E.] Wabash Coll, Dept Phys, Crawfordsville, IN 47933 USA.
[Krause, D. E.; Fischbach, E.; Jenkins, J. H.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Rogers, B. A.; Longuski, J. M.; Strange, N.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
[Buncher, J. B.] Wittenberg Univ, Dept Phys, Springfield, OH 45501 USA.
[Ging, A.; Strange, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jenkins, J. H.] Purdue Univ, Sch Nucl Engn, W Lafayette, IN 47907 USA.
[Sturrock, P. A.] Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA.
RP Krause, DE (reprint author), Wabash Coll, Dept Phys, Crawfordsville, IN 47933 USA.
EM kraused@wabash.edu
RI Krause, Dennis/O-3170-2013
FU USDOE [DE-AC02-76ER071428]; National Aeronautics and Space
Administration
FX The work of E.F. is supported in part by USDOE contract No.
DE-AC02-76ER071428. 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 38
TC 10
Z9 11
U1 2
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD AUG
PY 2012
VL 36
IS 1
BP 51
EP 56
DI 10.1016/j.astropartphys.2012.05.002
PG 6
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 020CT
UT WOS:000309787000009
ER
PT J
AU Moresco, M
Cimatti, A
Jimenez, R
Pozzetti, L
Zamorani, G
Bolzonella, M
Dunlop, J
Lamareille, F
Mignoli, M
Pearce, H
Rosati, P
Stern, D
Verde, L
Zucca, E
Carollo, CM
Contini, T
Kneib, JP
Le Fevre, O
Lilly, SJ
Mainieri, V
Renzini, A
Scodeggio, M
Balestra, I
Gobat, R
McLure, R
Bardelli, S
Bongiorno, A
Caputi, K
Cucciati, O
de la Torre, S
de Ravel, L
Franzetti, P
Garilli, B
Iovino, A
Kampczyk, P
Knobel, C
Kovac, K
Le Borgne, JF
Le Brun, V
Maier, C
Pello, R
Peng, Y
Perez-Montero, E
Presotto, V
Silverman, JD
Tanaka, M
Tasca, LAM
Tresse, L
Vergani, D
Almaini, O
Barnes, L
Bordoloi, R
Bradshaw, E
Cappi, A
Chuter, R
Cirasuolo, M
Coppa, G
Diener, C
Foucaud, S
Hartley, W
Kamionkowski, M
Koekemoer, AM
Lopez-Sanjuan, C
McCracken, HJ
Nair, P
Oesch, P
Stanford, A
Welikala, N
AF Moresco, M.
Cimatti, A.
Jimenez, R.
Pozzetti, L.
Zamorani, G.
Bolzonella, M.
Dunlop, J.
Lamareille, F.
Mignoli, M.
Pearce, H.
Rosati, P.
Stern, D.
Verde, L.
Zucca, E.
Carollo, C. M.
Contini, T.
Kneib, J. -P.
Le Fevre, O.
Lilly, S. J.
Mainieri, V.
Renzini, A.
Scodeggio, M.
Balestra, I.
Gobat, R.
McLure, R.
Bardelli, S.
Bongiorno, A.
Caputi, K.
Cucciati, O.
de la Torre, S.
de Ravel, L.
Franzetti, P.
Garilli, B.
Iovino, A.
Kampczyk, P.
Knobel, C.
Kovac, K.
Le Borgne, J. -F.
Le Brun, V.
Maier, C.
Pello, R.
Peng, Y.
Perez-Montero, E.
Presotto, V.
Silverman, J. D.
Tanaka, M.
Tasca, L. A. M.
Tresse, L.
Vergani, D.
Almaini, O.
Barnes, L.
Bordoloi, R.
Bradshaw, E.
Cappi, A.
Chuter, R.
Cirasuolo, M.
Coppa, G.
Diener, C.
Foucaud, S.
Hartley, W.
Kamionkowski, M.
Koekemoer, A. M.
Lopez-Sanjuan, C.
McCracken, H. J.
Nair, P.
Oesch, P.
Stanford, A.
Welikala, N.
TI Improved constraints on the expansion rate of the Universe up to z
similar to 1.1 from the spectroscopic evolution of cosmic chronometers
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE dark energy experiments; galaxy surveys
ID EARLY-TYPE GALAXIES; STELLAR POPULATION-MODELS; DIGITAL SKY SURVEY;
HUBBLE-SPACE-TELESCOPE; ELEMENT ABUNDANCE RATIOS; STAR-FORMATION
HISTORIES; HIGH-REDSHIFT GALAXIES; LUMINOUS RED GALAXIES; INITIAL MASS
FUNCTION; ORIGINS DEEP SURVEY
AB We present new improved constraints on the Hubble parameter H(z) in the redshift range 0.15 < z < 1.1, obtained from the differential spectroscopic evolution of early-type galaxies as a function of redshift. We extract a large sample of early-type galaxies ( 11000) from several spectroscopic surveys, spanning almost 8 billion years of cosmic lookback time (0.15 < z < 1.42). We select the most massive, red elliptical galaxies, passively evolving and without signature of ongoing star formation. Those galaxies can be used as standard cosmic chronometers, as firstly proposed by Jimenez & Loeb (2002), whose (life! Nit age evolution as a function of cosmic time directly probes H (z).
We analyze the 4000 angstrom break (D4000) as a function of redshift, use stellar population synthesis models to theoretically calibrate the dependence of the differential age evolution on the differential D4000, and estimate the Hubble parameter taking into account both statistical and systematical errors.
We provide 8 new measurements of H(z) (see table 4), and determine its change in H(z) to a precision of 5-12% mapping homogeneously the redshift range up to z 1.1; for the first time, we place a constraint on 11(z) at z not equal 0 with a precision comparable with the one achieved for the Hubble constant (about 5-6% at z similar to 0.2), and covered a redshift range (0.5 < z < 0.8) which is crucial to distinguish many different quintessence cosmologies.
These measurements have been tested to best match a ACDM model, clearly providing a statistically robust indication that the Universe is undergoing an accelerated expansion. This method shows the potentiality to open a new avenue in constrain a variety of alternative cosmologies, especially when future surveys (e.g. Euclid) will open the possibility to extend it up to z similar to 2.
C1 [Moresco, M.; Cimatti, A.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Jimenez, R.; Verde, L.] Univ Barcelona IEEC UB, ICREA, Barcelona 08028, Spain.
[Jimenez, R.; Verde, L.] Univ Barcelona IEEC UB, ICC, Barcelona 08028, Spain.
[Pozzetti, L.; Zamorani, G.; Bolzonella, M.; Mignoli, M.; Zucca, E.; Vergani, D.; Cappi, A.; Coppa, G.; Nair, P.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Dunlop, J.; Pearce, H.; McLure, R.; Caputi, K.; de la Torre, S.; de Ravel, L.; Cirasuolo, M.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Lamareille, F.; Contini, T.; Le Borgne, J. -F.; Pello, R.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Lamareille, F.; Contini, T.; Le Borgne, J. -F.; Pello, R.] Univ Toulouse, IRAP, UPS OMP, Toulouse, France.
[Rosati, P.; Mainieri, V.; Kovac, K.; Maier, C.] European So Observ, D-85748 Garching, Germany.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Carollo, C. M.; Lilly, S. J.; Kampczyk, P.; Knobel, C.; Peng, Y.; Barnes, L.; Bordoloi, R.; Diener, C.; Oesch, P.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Kneib, J. -P.; Le Fevre, O.; Balestra, I.; Le Brun, V.; Tasca, L. A. M.; Tresse, L.; Lopez-Sanjuan, C.] Univ Aix Marseille, Lab Astrophys Marseille, CNRS, F-13388 Marseille 13, France.
[Renzini, A.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Scodeggio, M.; Franzetti, P.; Garilli, B.] INAF IASF Milano, I-20133 Milan, Italy.
[Gobat, R.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA Saclay, CEA,DSM,CNRS,Irfu,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Balestra, I.; Bongiorno, A.; Coppa, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Cucciati, O.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Iovino, A.; Presotto, V.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy.
[Kovac, K.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Maier, C.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria.
[Perez-Montero, E.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Presotto, V.] Univ Insubria, I-22100 Como, Italy.
[Silverman, J. D.; Tanaka, M.] Univ Tokyo, IPMU, Kashiwa, Chiba 2778568, Japan.
[Vergani, D.] Ist Astrofis Spaziale & Fis Cosm Bologna, Ist Nazl Astrofis, I-40129 Bologna, Italy.
[Almaini, O.; Bradshaw, E.; Chuter, R.; Hartley, W.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Foucaud, S.] Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 11677, Taiwan.
[Kamionkowski, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[McCracken, H. J.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Oesch, P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Stanford, A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA.
[Welikala, N.] CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Welikala, N.] Univ Paris 11, F-91405 Orsay, France.
RP Moresco, M (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy.
EM michele.moresco@unibo.it
RI Kneib, Jean-Paul/A-7919-2015; Cappi, Alberto/O-9391-2015; Bardelli,
Sandro/O-9369-2015; Zucca, Elena/O-9396-2015; Mignoli,
Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015;
OI Kneib, Jean-Paul/0000-0002-4616-4989; Cappi,
Alberto/0000-0002-9200-7167; Bardelli, Sandro/0000-0002-8900-0298;
Zucca, Elena/0000-0002-5845-8132; Mignoli, Marco/0000-0002-9087-2835;
Bolzonella, Micol/0000-0003-3278-4607; Kamionkowski,
Marc/0000-0001-7018-2055; Pozzetti, Lucia/0000-0001-7085-0412;
Bongiorno, Angela/0000-0002-0101-6624; Jimenez,
Raul/0000-0002-3370-3103; Koekemoer, Anton/0000-0002-6610-2048; Iovino,
Angela/0000-0001-6958-0304; Balestra, Italo/0000-0001-9660-894X; Barnes,
Luke/0000-0002-0016-9485; Scodeggio, Marco/0000-0002-2282-5850;
Franzetti, Paolo/0000-0002-6986-0127; Vergani,
Daniela/0000-0003-0898-2216; Oesch, Pascal/0000-0001-5851-6649; Garilli,
Bianca/0000-0001-7455-8750
NR 100
TC 96
Z9 97
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD AUG
PY 2012
IS 8
AR 006
DI 10.1088/1475-7516/2012/08/006
PG 40
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 006DW
UT WOS:000308800700007
ER
PT J
AU Birn, J
Borovsky, JE
Hesse, M
AF Birn, J.
Borovsky, J. E.
Hesse, M.
TI The role of compressibility in energy release by magnetic reconnection
SO PHYSICS OF PLASMAS
LA English
DT Article
ID MAGNETOHYDRODYNAMIC TURBULENCE; MAGNETOTAIL; SIMULATIONS
AB Using resistive compressible magnetohydrodynamics, we investigate the energy release and transfer by magnetic reconnection in finite (closed or periodic) systems. The emphasis is on the magnitude of energy released and transferred to plasma heating in configurations that range from highly compressible to incompressible, based on the magnitude of the background beta (ratio of plasma pressure over magnetic pressure) and of a guide field in two-dimensional reconnection. As expected, the system becomes more incompressible, and the role of compressional heating diminishes, with increasing beta or increasing guide field. Nevertheless, compressional heating may dominate over Joule heating for values of the guide field of 2 or 3 (in relation to the reconnecting magnetic field component) and beta of 5-10. This result stems from the strong localization of the dissipation near the reconnection site, which is modeled based on particle simulation results. Imposing uniform resistivity, corresponding to a Lundquist number of 10(3) to 10(4), leads to significantly larger Ohmic heating. Increasing incompressibility greatly reduces the magnetic flux transfer and the amount of energy released, from similar to 10% of the energy associated with the reconnecting field component, for zero guide field and low beta, to similar to 0.2% - 0.4% for large values of the guide field B-y0 > 5 or large beta. The results demonstrate the importance of taking into account plasma compressibility and localization of dissipation in investigations of heating by turbulent reconnection, possibly relevant for solar wind or coronal heating. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4742314]
C1 [Birn, J.; Borovsky, J. E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA.
EM jbirn@spacescience.org
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU U.S. Department of Energy; NASA's Supporting Research and Technology
Program; MMS/SMART Program
FX This work was performed under the auspices of the U.S. Department of
Energy, supported by grants from NASA's Supporting Research and
Technology and MMS/SMART Programs. The authors acknowledge stimulating
discussions with S. Boldyrev and J. C. Perez.
NR 17
TC 7
Z9 7
U1 0
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD AUG
PY 2012
VL 19
IS 8
AR 082109
DI 10.1063/1.4742314
PG 9
WC Physics, Fluids & Plasmas
SC Physics
GA 012QV
UT WOS:000309252500013
ER
PT J
AU Passot, T
Sulem, RL
Hunana, P
AF Passot, T.
Sulem, R. L.
Hunana, P.
TI Extending magnetohydrodynamics to the slow dynamics of collisionless
plasmas
SO PHYSICS OF PLASMAS
LA English
DT Article
ID MAGNETIZED PLASMAS; FLUID; FLUCTUATIONS; EQUATIONS; WAVES; MODEL
AB A fluid approach aimed to provide a consistent description of the slow dynamics of a collisionless plasma, is presented. In this regime, both Landau damping and finite Larmor radius effects cannot be ignored. Two models are discussed; one retains the dynamics at sub-ionic scales, while the other is restricted to scales larger than the ion gyroscale. Special attention is paid to the capability of these approaches to accurately reproduce the properties of linear waves that are known to play an important role, for example, in the small-scale dynamics of solar wind turbulence. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4746092]
C1 [Passot, T.; Sulem, R. L.] Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, F-06304 Nice 4, France.
[Hunana, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Passot, T (reprint author), Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, BP 4229, F-06304 Nice 4, France.
FU European Commission [284515]; INSU-CNRS; International Space Science
Institute in Bern; OCA; NASA
FX The research leading to these results has received funding from the
European Commission's Seventh Framework Programme (FP7/2007-2013) under
the grant agreement SHOCK (Project No. 284515). The support of INSU-CNRS
"Programme Soleil-Terre" is also acknowledged. We thank ISSI team 185
"Dispersive cascade and dissipation in collisionless space plasma
turbulence-observations and simulations" under leadership of E.
Yordanova and financed by the International Space Science Institute in
Bern. P.H. was supported by the OCA Poincare fellowship and by the NASA
Postdoctoral Fellowship (administered by ORAU).
NR 22
TC 15
Z9 16
U1 0
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD AUG
PY 2012
VL 19
IS 8
AR 082113
DI 10.1063/1.4746092
PG 15
WC Physics, Fluids & Plasmas
SC Physics
GA 012QV
UT WOS:000309252500017
ER
PT J
AU Schindler, K
Birn, J
Hesse, M
AF Schindler, K.
Birn, J.
Hesse, M.
TI Kinetic model of electric potentials in localized collisionless plasma
structures under steady quasi-gyrotropic conditions
SO PHYSICS OF PLASMAS
LA English
DT Article
ID THIN CURRENT SHEETS; SUBSTORM GROWTH-PHASE; PARTICLE-ACCELERATION;
MAGNETIC RECONNECTION; MAGNETOTAIL; CLUSTER; FIELDS
AB Localized plasma structures, such as thin current sheets, generally are associated with localized magnetic and electric fields. In space plasmas localized electric fields not only play an important role for particle dynamics and acceleration but may also have significant consequences on larger scales, e.g., through magnetic reconnection. Also, it has been suggested that localized electric fields generated in the magnetosphere are directly connected with quasi-steady auroral arcs. In this context, we present a two-dimensional model based on Vlasov theory that provides the electric potential for a large class of given magnetic field profiles. The model uses an expansion for small deviation from gyrotropy and besides quasineutrality it assumes that electrons and ions have the same number of particles with their generalized gyrocenter on any given magnetic field line. Specializing to one dimension, a detailed discussion concentrates on the electric potential shapes (such as "U" or "S" shapes) associated with magnetic dips, bumps, and steps. Then, it is investigated how the model responds to quasi-steady evolution of the plasma. Finally, the model proves useful in the interpretation of the electric potentials taken from two existing particle simulations. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4747162]
C1 [Schindler, K.] Ruhr Univ Bochum, D-44780 Bochum, Germany.
[Birn, J.] Space Sci Inst, Boulder, CO 80301 USA.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schindler, K (reprint author), Ruhr Univ Bochum, D-44780 Bochum, Germany.
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU U.S. Department of Energy; NASA [NNG08EJ63I, NNH10A045I, NNH11AQ42I];
NASA's MMS mission
FX The work of J.B. was performed at Los Alamos National Laboratory, under
the auspices of the U.S. Department of Energy with support by NASA
through Grant Nos. NNG08EJ63I, NNH10A045I, and NNH11AQ42I. The work of
M.H. was supported by NASA's MMS mission.
NR 43
TC 16
Z9 16
U1 0
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD AUG
PY 2012
VL 19
IS 8
AR 082904
DI 10.1063/1.4747162
PG 8
WC Physics, Fluids & Plasmas
SC Physics
GA 012QV
UT WOS:000309252500074
ER
PT J
AU Veraverbeke, S
Hook, S
Hulley, G
AF Veraverbeke, S.
Hook, S.
Hulley, G.
TI An alternative spectral index for rapid fire severity assessments
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Fire severity; Normalized Burn Ratio (NBR); Mid infrared; Moderate
Resolution Imaging Spectroradiometer (MODIS); Advanced Spaceborne and
Thermal Emission Radiometer (ASTER); Hyperspectral Infrared Imager
(HyspIRI)
ID NORMALIZED BURN RATIO; 2007 PELOPONNESE WILDFIRES; LANDSAT THEMATIC
MAPPER; REMOTELY-SENSED DATA; VEGETATION; MODELS; GREECE; DNBR;
REGENERATION; REFLECTANCE
AB Rapid fire severity assessments are essential for timely post-fire rehabilitation responses. The Landsat differenced Normalized Burn Ratio (dNBR) has become the standard spectral index for assessing fire severity. The dNBR is generally calculated using the first available cloud-free post-fire image and a pre-fire image. This bitemporal image differencing can be problematic due to image-to-image differences in illumination and phenology for example. We have developed an alternative index based on single date short-wave infrared (SWIR) and mid infrared (MIR) reflectance. In contrast with the (d)NBR, the SWIR-MIR index (SMI) is robust against scattering caused by smoke plumes over active fires allowing fire severity assessments to be generated when the area is still obscured by smoke. The SMI was generated using MODIS/ASTER (MASTER) airborne simulator data acquired over the recent 2011 Wallow fire in Arizona, USA. Simulation experiments showed that the SMI is more sensitive to char fractional cover than the NBR. We performed a regression analysis in which 92 Geo Composite Burn Index (GeoCBI) field plots of severity were randomly assigned to two equal halves, a training and a validation dataset, during ten separate trials. The SMI performed better to estimate GeoCBI values than the NBR (SMI R-2=0.69 +/- 0.06 and NBR R-2=0.60 +/- 0.06). The dNBR demonstrated slightly better performance than the SMI (dNBR R-2= 0.71 +/- 0.05), however this difference was not significant at the 95% confidence level. Although no spaceborne sensors with pixel sizes smaller than 100 m currently offer the possibility of a SWIR-MIR band combination, the airborne results illustrate the potential of this band combination for the remote sensing of post-fire effects. Such data will become available with the advent of the next generation satellite sensors, such as the planned spaceborne Hyperspectral Infrared Imager (HyspIRI). (C) 2012 Published by Elsevier Inc.
C1 [Veraverbeke, S.; Hook, S.; Hulley, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Veraverbeke, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sander.S.Veraverbeke@jpl.nasa.gov; Simon.J.Hook@jpl.nasa.gov;
Glynn.Hulley@jpl.nasa.gov
RI Veraverbeke, Sander/H-2301-2012
OI Veraverbeke, Sander/0000-0003-1362-5125
FU National Aeronautics and Space Administration; NASA grant for
Interdisciplinary Research in Earth Science
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. The
work was funded by a NASA grant for Interdisciplinary Research in Earth
Science awarded to Dr. Yufang Jin. We would like to thank the anonymous
reviewers for their useful suggestions to improve the manuscript.
Copyright 2012 California Institute of Technology. Government
sponsorship acknowledged.
NR 61
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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 AUG
PY 2012
VL 123
BP 72
EP 80
DI 10.1016/j.rse.2012.02.025
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 016CX
UT WOS:000309496000006
ER
PT J
AU Liang, YL
Colgan, W
Lv, Q
Steffen, K
Abdalati, W
Stroeve, J
Gallaher, D
Bayou, N
AF Liang, Yu-Li
Colgan, William
Lv, Qin
Steffen, Konrad
Abdalati, Waleed
Stroeve, Julienne
Gallaher, David
Bayou, Nicolas
TI A decadal investigation of supraglacial lakes in West Greenland using a
fully automatic detection and tracking algorithm
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Change detection; Temporal tracking; MODIS; Greenland Ice Sheet;
Supraglacial lake; Melt intensity
ID ICE-SHEET; SEASONAL EVOLUTION; MELT; GLACIER; ACCELERATION; DRAINAGE;
DRIVEN; ISBRAE
AB The sudden drainage of supraglacial lakes has been previously observed to initiate surface-to-bed hydrologic connections, which are capable of enhancing basal sliding, in regions of the Greenland Ice Sheet where ice thickness approaches 1 km. In this study, we develop a robust algorithm, which automatically detects and tracks individual supraglacial lakes using visible satellite imagery, to document the evolution of a population of West Greenland supraglacial lakes over ten consecutive melt seasons. Validation tests indicate that the algorithm is highly accurate: 99.0% of supraglacial lakes can be detected and tracked and 96.3% of reported lakes are true supraglacial lakes with accurate lake properties, such as lake area, and timing of formation and drainage. Investigation of the interannual evolution of supraglacial lakes in the context of annual melt intensity reveals that during more intense melt years, supraglacial lakes drain more frequently and earlier in the melt season. Additionally, the lake population extends to higher elevations during more intense melt years, exposing an increased inland area of the ice sheet to sudden lake drainage events. These observations suggest that increased surface meltwater production due to climate change will enhance the spatial extent and temporal frequency of lake drainage events. It is unclear whether this will ultimately increase or decrease the basal sliding sensitivity of interior regions of the Greenland Ice Sheet. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Liang, Yu-Li; Lv, Qin] Univ Colorado, Dept Comp Sci, Boulder, CO 80309 USA.
[Colgan, William; Steffen, Konrad; Abdalati, Waleed; Stroeve, Julienne; Gallaher, David; Bayou, Nicolas] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Steffen, Konrad; Abdalati, Waleed; Bayou, Nicolas] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Abdalati, Waleed] NASA, Washington, DC 20546 USA.
[Stroeve, Julienne; Gallaher, David] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
RP Liang, YL (reprint author), Univ Colorado, Dept Comp Sci, Boulder, CO 80309 USA.
EM Yu-Li.Liang@colorado.edu; William.Colgan@colorado.edu;
Qin.Lv@colorado.edu; Konrad.Steffen@colorado.edu;
Waleed.Abdalati@colorado.edu; Stroeve@nsidc.org;
David.Gallaher@nsidc.org; Nicolas.Bayou@colorado.edu
RI Colgan, William/H-1570-2014; Steffen, Konrad/C-6027-2013
OI Colgan, William/0000-0001-6334-1660; Steffen, Konrad/0000-0001-8658-1026
FU National Science Foundation (NSF) [ARC 0941442]; Natural Science and
Engineering Research Council (NSERC) of Canada; Cooperative Institute
for Research in Environmental Sciences (CIRES)
FX This work was supported by the National Science Foundation (NSF) grant
ARC 0941442 to J.S.. D.G. and Q.L. We thank the National Aeronautics and
Space Administration (NASA) for freely providing MODIS data from the
Warehouse Inventory Search Tool (WIST). Y.L. thanks David Fanning for
his advice and assistance during the early stages of this project. W.C.
thanks the Natural Science and Engineering Research Council (NSERC) of
Canada and the Cooperative Institute for Research in Environmental
Sciences (CIRES) for fellowship support. We thank Doug MacAyeal for an
insightful collegial review of an earlier version of this manuscript.
NR 38
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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 AUG
PY 2012
VL 123
BP 127
EP 138
DI 10.1016/j.rse.2012.03.020
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 016CX
UT WOS:000309496000012
ER
PT J
AU Jones, MO
Kimball, JS
Jones, LA
McDonald, KC
AF Jones, Matthew O.
Kimball, John S.
Jones, Lucas A.
McDonald, Kyle C.
TI Satellite passive microwave detection of North America start of season
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Phenology; VOD; AMSR-E; MODIS; NACP; NDVI; LAI; TIMESAT; Start of season
ID PRECIPITATION PULSES; CROP RESIDUE; TIME-SERIES; AMSR-E; PHENOLOGY;
CLIMATE; FOREST; BACKSCATTER; COVER; INDEX
AB The start of season (SOS) phenological metric indicates the seasonal onset of vegetation activity, including canopy growth, photosynthesis and associated increases in land-atmosphere water, energy and carbon (CO2) exchanges influencing weather and climate variability. Satellite optical-infrared (IR) remote sensing is responsive to vegetation greenness and SOS, but measurement accuracy and global monitoring are constrained by atmosphere cloud/aerosol contamination and seasonal decreases in solar illumination for many areas. The vegetation optical depth (VOD) parameter from satellite passive microwave remote sensing provides an alternative means for global phenology monitoring that is sensitive to vegetation canopy biomass and water content, and insensitive to atmosphere and solar illumination constraints. A global VOD record from the Advanced Microwave Scanning Radiometer for EOS (AMSR-E) was used to estimate North America SOS patterns and annual variability at the ecoregion scale. The SOS metrics were derived for a four year (2004-2007) record using TIMESAT and AMSR-E 10.7 GHz frequency VOD retrievals composited to 4-day median time series. The VOD SOS corresponded favorably with MODIS-for-NACP NDVI (0.73 2 R-circle plus we measure an occurrence of less than 0.001 planets per star. For all planets with orbital periods less than 50 days, we measure occurrence of 0.130 +/- 0.008, 0.023 +/- 0.003, and 0.013 +/- 0.002 planets per star for planets with radii 2-4, 4-8, and 8-32 R-circle plus, in agreement with Doppler surveys. We fit occurrence as a function of P to a power-law model with an exponential cutoff below a critical period P-0. For smaller planets, P-0 has larger values, suggesting that the "parking distance" for migrating planets moves outward with decreasing planet size. We also measured planet occurrence over a broader stellar T-eff range of 3600-7100 K, spanning M0 to F2 dwarfs. Over this range, the occurrence of 2-4 R-circle plus planets in the Kepler field increases with decreasing T-eff, with these small planets being seven times more abundant around cool stars (3600-4100 K) than the hottest stars in our sample (6600-7100 K).
C1 [Howard, Andrew W.; Marcy, Geoffrey W.; Basri, Gibor S.; Isaacson, Howard; Walkowicz, Lucianne M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Jenkins, Jon M.; Van Cleve, Jeffrey; Caldwell, Douglas A.; Tarter, Jill; Machalek, Pavel; Tenenbaum, Peter; Twicken, Joseph D.; Devore, Edna; Smith, Jeffrey C.; Morris, Robert L.; Thompson, Susan E.; Mullally, Fergal] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Latham, David W.; Torres, Guillermo; Fressin, Francois; Sasselov, Dimitar D.; Charbonneau, David; Dupree, Andrea; Holman, Matthew J.; Ragozzine, Darin; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brown, Timothy M.; Shporer, Avi] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark.
[Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Seager, Sara; Rogers, Leslie] MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, Cambridge, MA 02139 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Fabrycky, Daniel C.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06510 USA.
[Ford, Eric B.; Moorhead, Althea V.; Morehead, Robert C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Girouard, Forrest R.; Klaus, Todd C.; Morton, Timothy D.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91109 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Lucas, Philip W.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
RP Howard, AW (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM howard@astro.berkeley.edu
RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; Howard,
Andrew/D-4148-2015;
OI Caldwell, Douglas/0000-0003-1963-9616; Howard,
Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354;
Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; /0000-0001-6545-639X; Fischer,
Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183
FU NASA [NNX06AH52G]; National Center for Atmospheric Research; National
Science Foundation; NASA's Science Mission Directorate
FX We thank E. Chiang and H. Knutson for helpful conversations. We
gratefully acknowledge D. Monet and many other members of the Kepler
team. We thank the W. M. Keck Observatory, and both NASA and the
University of California for the use of the Keck telescope. We are
grateful to the Keck technical staff, especially S. Dahm, H. Tran, and
G. Hill for the support of Keck instrumentation, and R. Kibrick, G.
Wirth, R. Goodrich for the support of remote observing. We extend
special thanks to those of Hawaiian ancestry on whose sacred mountain of
Mauna Kea we are privileged to be guests. G. M. acknowledges NASA grant
NNX06AH52G. J.C.-D. acknowledges support from the National Center for
Atmospheric Research, which is sponsored by the National Science
Foundation. Funding for the Kepler Discovery mission is provided by
NASA's Science Mission Directorate.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2012
VL 201
IS 2
AR 15
DI 10.1088/0067-0049/201/2/15
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016YN
UT WOS:000309555900008
ER
PT J
AU Kospal, A
Abraham, P
Acosta-Pulido, JA
Dullemond, CP
Henning, T
Kun, M
Leinert, C
Moor, A
Turner, NJ
AF Kospal, A.
Abraham, P.
Acosta-Pulido, J. A.
Dullemond, C. P.
Henning, Th
Kun, M.
Leinert, Ch
Moor, A.
Turner, N. J.
TI MID-INFRARED SPECTRAL VARIABILITY ATLAS OF YOUNG STELLAR OBJECTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; infrared: stars; methods: data analysis; stars:
pre-main sequence; techniques: spectroscopic
ID HERBIG-AE/BE-STARS; PRE-MAIN-SEQUENCE; T-TAURI STARS; VEGA-LIKE SYSTEMS;
POLYCYCLIC AROMATIC-HYDROCARBONS; MILLIMETER-WAVE PROPERTIES; DISK
SURROUNDING HD-142527; NEARBY MOLECULAR CLOUDS; SPITZER-SPACE-TELESCOPE;
RHO-OPHIUCHI CLOUD
AB Optical and near-infrared variability is a well-known property of young stellar objects. However, a growing number of recent studies claim that a considerable fraction of them also exhibit mid-infrared flux changes. With the aim of studying and interpreting variability on a decadal timescale, here we present a mid-infrared spectral atlas containing observations of 68 low-and intermediate-mass young stellar objects. The atlas consists of 2.5-11.6 mu m low-resolution spectra obtained with the ISOPHOT-S instrument on board the Infrared Space Observatory (ISO) between 1996 and 1998, as well as 5.2-14.5 mu m low-resolution spectra obtained with the Infrared Spectrograph instrument on board the Spitzer Space Telescope between 2004 and 2007. The observations were retrieved from the ISO and Spitzer archives and were post-processed interactively by our own routines. For those 47 objects where multi-epoch spectra were available, we analyze mid-infrared spectral variability on annual and/or decadal timescales. We identify 37 variable candidate sources. Many stars show wavelength-independent flux changes, possibly due to variable accretion rates. In several systems, all exhibiting 10 mu m silicate emission, the variability of the 6-8 mu m continuum, and the silicate feature exhibit different amplitudes. A possible explanation is variable shadowing of the silicate-emitting region by an inner disk structure of changing height or extra silicate emission from dust clouds in the disk atmosphere. Our results suggest that mid-infrared variability, in particular, the wavelength-dependent changes, is more ubiquitous than was known before. Interpreting this variability is a new possibility for exploring the structure of the disk and its dynamical processes.
C1 [Kospal, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Kospal, A.] European Space Agcy, Estec, SRE SA, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands.
[Abraham, P.; Kun, M.; Moor, A.] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, H-1525 Budapest, Hungary.
[Acosta-Pulido, J. A.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Acosta-Pulido, J. A.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
[Dullemond, C. P.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Dullemond, C. P.; Henning, Th; Leinert, Ch] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Turner, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kospal, A (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM akospal@rssd.esa.int
OI Dullemond, Cornelis/0000-0002-7078-5910
FU ESA; ISAS; NASA; Netherlands Organization for Scientific Research (NWO);
Hungarian Scientific Research Fund [OTKA-101393]
FX This work is based on observations made with the Infrared Space
Observatory (ISO) and with the Spitzer Space Telescope. ISO is an ESA
project with instruments funded by ESA Member States (especially the PI
countries: France, Germany, the Netherlands, and UK) and with the
participation of ISAS and NASA. Spitzer is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA.; We thank the anonymous referee for providing a
thorough and very helpful report. The ISOPHOT data presented in this
paper were reduced using the ISOPHOT Interactive Analysis package PIA,
which is a joint development by the ESA Astrophysics Division and the
ISOPHOT Consortium, lead by the Max-Planck-Institut fur Astronomie
(MPIA). This research has made use of the SIMBAD database, operated at
CDS, Strasbourg, France, NASA's Astrophysics Data System, and the
NASA/IPAC Infrared Science Archive, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA. A.K. acknowledges support from the Netherlands
Organization for Scientific Research (NWO). This work was partly
supported by the grant OTKA-101393 of the Hungarian Scientific Research
Fund.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2012
VL 201
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AR 11
DI 10.1088/0067-0049/201/2/11
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016YN
UT WOS:000309555900004
ER
PT J
AU McNally, CP
Lyra, W
Passy, JC
AF McNally, Colin P.
Lyra, Wladimir
Passy, Jean-Claude
TI A WELL-POSED KELVIN-HELMHOLTZ INSTABILITY TEST AND COMPARISON
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE hydrodynamics; instabilities; methods: numerical
ID SMOOTHED PARTICLE HYDRODYNAMICS; STABILITY; SIMULATIONS; TURBULENCE;
TRANSPORT; GALAXIES; MESH; SPH; MHD
AB Recently, there has been a significant level of discussion of the correct treatment of Kelvin-Helmholtz instability (KHI) in the astrophysical community. This discussion relies largely on how the KHI test is posed and analyzed. We pose a stringent test of the initial growth of the instability. The goal is to provide a rigorous methodology for verifying a code on two-dimensional KHI. We ran the problem in the Pencil Code, Athena, Enzo, NDSPMHD, and Phurbas. A strict comparison, judgment, or ranking, between codes is beyond the scope of this work, though this work provides the mathematical framework needed for such a study. Nonetheless, how the test is posed circumvents the issues raised by tests starting from a sharp contact discontinuity yet it still shows the poor performance of smoothed particle hydrodynamics (SPH). We then comment on the connection between this behavior to the underlying lack of zeroth-order consistency in SPH interpolation. We comment on the tendency of some methods, particularly those with very low numerical diffusion, to produce secondary Kelvin-Helmholtz billows on similar tests. Though the lack of a fixed, physical diffusive scale in the Euler equations lies at the root of the issue, we suggest that in some methods an extra diffusion operator should be used to damp the growth of instabilities arising from grid noise. This statement applies particularly to moving-mesh tessellation codes, but also to fixed-grid Godunov schemes.
C1 [McNally, Colin P.; Lyra, Wladimir; Passy, Jean-Claude] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[McNally, Colin P.] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Lyra, Wladimir] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Passy, Jean-Claude] Univ Victoria, Dept Phys & Astron, Victoria, BC, Canada.
RP McNally, CP (reprint author), Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
EM cmcnally@amnh.org; wlyra@jpl.nasa.gov; jcpassy@uvic.ca
RI McNally, Colin/C-4336-2015
OI McNally, Colin/0000-0002-2565-6626
FU National Science Foundation (NSF) [AST-0835734, AST-0607111,
AST-1009802, OCI-1053575]
FX We are indebted to the authors of NDSPMHD, Athena, Enzo, and the Pencil
Code for making the codes freely available to us. The SPH visualizations
were created with SPLASH (Price 2007). We thank the anonymous referee
for constructive comments that significantly improved the organization
of the paper. We thank Daniel Price for feedback on a draft of this
manuscript, and suggesting the use of fully relaxed SPH initial
conditions and the isodensity special case. We thank Mordecai-Mark Mac
Low for his support and useful discussions. We thank Paul Duffel for
useful discussions about moving-mesh schemes. J-C.P. thanks Orsola De
Marco and Falk Herwig for their support. This work has been supported by
National Science Foundation (NSF) grants AST-0835734 and AST-0607111. W.
L. gratefully acknowledges partial financial support from the NSF under
grant No. AST-1009802. W. L. completed co-writing this work at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
work used the Extreme Science and Engineering Discovery Environment
(XSEDE), which is supported by National Science Foundation grant No.
OCI-1053575. This work used computer time provided partially by Westgrid
and Compute Canada.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2012
VL 201
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AR 18
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PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016YN
UT WOS:000309555900011
ER
PT J
AU Vaillancourt, JE
Matthews, BC
AF Vaillancourt, John E.
Matthews, Brenda C.
TI SUBMILLIMETER POLARIZATION OF GALACTIC CLOUDS: A COMPARISON OF 350 mu m
AND 850 mu m DATA
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE dust, extinction; ISM: clouds; polarization; submillimeter: ISM
ID FORMING MOLECULAR CLOUDS; MAGNETIC-FIELD STRUCTURE; CLERK MAXWELL
TELESCOPE; GRAIN ALIGNMENT; RADIATIVE TORQUES; INTERSTELLAR DUST;
INFRARED POLARIZATION; IMAGING POLARIMETRY; LINEAR-POLARIZATION; ARRAY
POLARIMETRY
AB The Hertz and SCUBA polarimeters, working at 350 mu m and 850 mu m, respectively, have measured the polarized emission in scores of Galactic clouds. Of the clouds in each data set, 17 were mapped by both instruments with good polarization signal-to-noise ratios. We present maps of each of these 17 clouds comparing the dual-wavelength polarization amplitudes and position angles at the same spatial locations. In total number of clouds compared, this is a four-fold increase over previous work. Across the entire data set real position angle differences are seen between wavelengths. While the distribution of phi(850)-phi(350) is centered near zero (near-equal angles), 64% of data points with high polarization signal-to-noise (P >= 3 sigma(p)) have vertical bar phi(850)-phi(350)vertical bar > 10 degrees. Of those data with small changes in position angle (<= 10 degrees) the median ratio of the polarization amplitudes is P(850)/P(350) = 1.7 +/- 0.6. This value is consistent with previous work performed on smaller samples and models that require mixtures of different grain properties and polarization efficiencies. Along with the polarization data we have also compiled the intensity data at both wavelengths; we find a trend of decreasing polarization with increasing 850-to-350 mu m intensity ratio. All the polarization and intensity data presented here (1699 points in total) are available in electronic format.
C1 [Vaillancourt, John E.] NASA, SOFIA Sci Ctr, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Matthews, Brenda C.] Natl Res Council Canada, Herzberg Inst, Victoria, BC V9E 2E7, Canada.
RP Vaillancourt, JE (reprint author), NASA, SOFIA Sci Ctr, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jvaillancourt@sofia.usra.edu; brenda.matthews@nrc-cnrc.gc.ca
OI Vaillancourt, John/0000-0001-8916-1828
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2012
VL 201
IS 2
AR 13
DI 10.1088/0067-0049/201/2/13
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016YN
UT WOS:000309555900006
ER
PT J
AU Wilson-Hodge, CA
Case, GL
Cherry, ML
Rodi, J
Camero-Arranz, A
Jenke, P
Chaplin, V
Beklen, E
Finger, M
Bhat, N
Briggs, MS
Connaughton, V
Greiner, J
Kippen, RM
Meegan, CA
Paciesas, WS
Preece, R
von Kienlin, A
AF Wilson-Hodge, Colleen A.
Case, Gary L.
Cherry, Michael L.
Rodi, James
Camero-Arranz, Ascension
Jenke, Peter
Chaplin, Vandiver
Beklen, Elif
Finger, Mark
Bhat, Narayan
Briggs, Michael S.
Connaughton, Valerie
Greiner, Jochen
Kippen, R. Marc
Meegan, Charles A.
Paciesas, William S.
Preece, Robert
von Kienlin, Andreas
TI THREE YEARS OF FERMI GBM EARTH OCCULTATION MONITORING: OBSERVATIONS OF
HARD X-RAY/SOFT GAMMA-RAY SOURCES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma rays: general; methods: data analysis; occultations;
surveys; X-rays: stars
ID LARGE-AREA TELESCOPE; BURST MONITOR; CRAB-NEBULA; LUNAR OCCULTATION;
CATALOG; BINARY; EMISSION; MASS; X-1; CALIBRATION
AB The Gamma-ray Burst Monitor (GBM) on board Fermi has been providing continuous data to the astronomical community since 2008 August 12. In this paper, we present the results of the analysis of the first three years of these continuous data using the Earth occultation technique to monitor a catalog of 209 sources. From this catalog, we detect 99 sources, including 40 low-mass X-ray binary/neutron star systems, 31 high-mass X-ray binary/neutron star systems, 12 black hole binaries, 12 active galaxies, and 2 other sources, plus the Crab Nebula, and the Sun. Nine of these sources are detected in the 100-300 keV band, including seven black hole binaries, the active galaxy Cen A, and the Crab. The Crab and Cyg X-1 are also detected in the 300-500 keV band. GBM provides complementary data to other sky-monitors below 100 keV and is the only all-sky monitor above 100 keV. Up-to-date light curves for all of the catalog sources can be found online.
C1 [Wilson-Hodge, Colleen A.; Jenke, Peter] NASA, George C Marshall Space Flight Ctr, ZP Astrophys Off 12, Huntsville, AL 35812 USA.
[Case, Gary L.; Cherry, Michael L.; Rodi, James] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Camero-Arranz, Ascension] Inst Ciencias Espacio IEEC CSIC, Barcelona 08193, Spain.
[Chaplin, Vandiver; Bhat, Narayan; Briggs, Michael S.; Connaughton, Valerie; Preece, Robert] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Beklen, Elif] Suleyman Demirel Univ, Dept Phys, TR-32260 Isparta, Turkey.
[Finger, Mark; Paciesas, William S.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Greiner, Jochen; Meegan, Charles A.; von Kienlin, Andreas] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kippen, R. Marc] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Wilson-Hodge, CA (reprint author), NASA, George C Marshall Space Flight Ctr, ZP Astrophys Off 12, Huntsville, AL 35812 USA.
OI Preece, Robert/0000-0003-1626-7335
FU NASA Fermi Guest Investigator program; NASA/Louisiana Board of Regents
Cooperative Agreement [NNX07AT62A (LSU)]; Louisiana Board of Regents
Graduate Fellowship Program; NOAA Space Prediction Center helpdesk
FX This work is supported by the NASA Fermi Guest Investigator program,
NASA/Louisiana Board of Regents Cooperative Agreement NNX07AT62A (LSU),
and the Louisiana Board of Regents Graduate Fellowship Program (J.R.).
We thank the NOAA Space Prediction Center helpdesk for their support and
Sebastian Drave for providing information about SFXT systems with known
orbital solutions. Flare database entries and Swift/BAT comparisons
relied upon Swift/BAT transient monitor results provided by the
Swift/BAT team. This research has made use of the MAXI data provided by
RIKEN, JAXA, and the MAXI team and results provided by the RXTE/ASM
teams at MIT and GSFC.
NR 49
TC 10
Z9 10
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2012
VL 201
IS 2
AR 33
DI 10.1088/0067-0049/201/2/33
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016YN
UT WOS:000309555900026
ER
PT J
AU Tsou, P
Brownlee, DE
McKay, CP
Anbar, AD
Yano, H
Altwegg, K
Beegle, LW
Dissly, R
Strange, NJ
Kanik, I
AF Tsou, Peter
Brownlee, Donald E.
McKay, Christopher P.
Anbar, Ariel D.
Yano, Hajime
Altwegg, Kathrin
Beegle, Luther W.
Dissly, Richard
Strange, Nathan J.
Kanik, Isik
TI LIFE: Life Investigation For Enceladus A Sample Return Mission Concept
in Search for Evidence of Life
SO ASTROBIOLOGY
LA English
DT Article
DE Astrobiology; Habitability; Enceladus; Biosignatures
ID COMET 81P/WILD-2; STARDUST; PLUME; WATER; RING; ATMOSPHERE; MOLECULES;
SATURN; DUST; GAS
AB Life Investigation For Enceladus (LIFE) presents a low-cost sample return mission to Enceladus, a body with high astrobiological potential. There is ample evidence that liquid water exists under ice coverage in the form of active geysers in the "tiger stripes" area of the southern Enceladus hemisphere. This active plume consists of gas and ice particles and enables the sampling of fresh materials from the interior that may originate from a liquid water source. The particles consist mostly of water ice and are 1-10 mu in diameter. The plume composition shows H2O, CO2, CH4, NH3, Ar, and evidence that more complex organic species might be present. Since life on Earth exists whenever liquid water, organics, and energy coexist, understanding the chemical components of the emanating ice particles could indicate whether life is potentially present on Enceladus. The icy worlds of the outer planets are testing grounds for some of the theories for the origin of life on Earth.
The LIFE mission concept is envisioned in two parts: first, to orbit Saturn (in order to achieve lower sampling speeds, approaching 2 km/s, and thus enable a softer sample collection impact than Stardust, and to make possible multiple flybys of Enceladus); second, to sample Enceladus' plume, the E ring of Saturn, and the Titan upper atmosphere. With new findings from these samples, NASA could provide detailed chemical and isotopic and, potentially, biological compositional context of the plume. Since the duration of the Enceladus plume is unpredictable, it is imperative that these samples are captured at the earliest flight opportunity. If LIFE is launched before 2019, it could take advantage of a Jupiter gravity assist, which would thus reduce mission lifetimes and launch vehicle costs. The LIFE concept offers science returns comparable to those of a Flagship mission but at the measurably lower sample return costs of a Discovery-class mission.
C1 [Brownlee, Donald E.] Univ Washington, Seattle, WA 98195 USA.
[McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Anbar, Ariel D.] Arizona State Univ, Tempe, AZ USA.
[Yano, Hajime] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Tokyo, Japan.
[Altwegg, Kathrin] Univ Bern, Bern, Switzerland.
[Beegle, Luther W.; Strange, Nathan J.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dissly, Richard] Ball Aerosp & Technol Corp, Boulder, CO USA.
EM Tsou.Peter@gmail.com; Isik.Kanik@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); NASA Astrobiology
Institute Icy Worlds; JPL Planetary Exploration Office
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract from the National
Aeronautics and Space Administration (NASA). We gratefully acknowledge
the financial support from the NASA Astrobiology Institute Icy Worlds
and the JPL Planetary Exploration Office.
NR 61
TC 13
Z9 13
U1 4
U2 75
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD AUG
PY 2012
VL 12
IS 8
BP 730
EP 742
DI 10.1089/ast.2011.0813
PG 13
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 006IA
UT WOS:000308811500003
PM 22970863
ER
PT J
AU Xu, J
Campbell, JM
Zhang, NL
Hickey, WJ
Sahai, N
AF Xu, Jie
Campbell, Jay M.
Zhang, Nianli
Hickey, William J.
Sahai, Nita
TI Did Mineral Surface Chemistry and Toxicity Contribute to Evolution of
Microbial Extracellular Polymeric Substances?
SO ASTROBIOLOGY
LA English
DT Article
DE Mineral toxicity; Bacteria; EPS evolution; Biofilms; Cytotoxicity;
Silica; Anatase; Alumina
ID BIOFILM FORMATION; PSEUDOMONAS-AERUGINOSA; SILICATE COMPLEXES; BACTERIA;
OXYGEN; SYSTEMS; NANOPARTICLES; ENVIRONMENT; MECHANISMS; OXIDATION
AB Modern ecological niches are teeming with an astonishing diversity of microbial life in biofilms closely associated with mineral surfaces, which highlights the remarkable success of microorganisms in conquering the challenges and capitalizing on the benefits presented by the mineral-water interface. Biofilm formation capability likely evolved on early Earth because biofilms provide crucial cell survival functions. The potential toxicity of mineral surfaces toward cells and the complexities of the mineral-water-cell interface in determining the toxicity mechanisms, however, have not been fully appreciated. Here, we report a previously unrecognized role for extracellular polymeric substances (EPS), which form biofilms in shielding cells against the toxicity of mineral surfaces. Using colony plating and LIVE/DEAD staining methods in oxide suspensions versus oxide-free controls, we found greater viability of wild-type, EPS-producing strains of Pseudomonas aeruginosa PAO1 compared to their isogenic knockout mutant with defective biofilm-producing capacity. Oxide toxicity was specific to its surface charge and particle size. High resolution transmission electron microscopy (HRTEM) images and assays for highly reactive oxygen species (hROS) on mineral surfaces suggested that EPS shield via both physical and chemical mechanisms. Intriguingly, qualitative as well as quantitative measures of EPS production showed that toxic minerals induced EPS production in bacteria. By determining the specific toxicity mechanisms, we provide insight into the potential impact of mineral surfaces in promoting increased complexity of cell surfaces, including EPS and biofilm formation, on early Earth.
C1 [Sahai, Nita] Univ Akron, Dept Polymer Sci, Akron, OH 44313 USA.
[Sahai, Nita] Univ Akron, NASA Astrobiol Inst, Akron, OH 44313 USA.
[Xu, Jie; Sahai, Nita] Univ Wisconsin, Dept Geosci, Madison, WI USA.
[Xu, Jie; Sahai, Nita] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI USA.
[Campbell, Jay M.] Univ Wisconsin, Dept Biochem, Madison, WI 53705 USA.
[Zhang, Nianli; Sahai, Nita] Univ Wisconsin, Mat Sci Program, Madison, WI 53706 USA.
[Xu, Jie] George Washington Univ, Dept Chem, Washington, DC 20052 USA.
[Zhang, Nianli] Univ Michigan, Sch Dent, Dept Biol & Mat Sci, Ann Arbor, MI 48109 USA.
[Hickey, William J.] Univ Wisconsin, Dept Soil Sci, Madison, WI 53706 USA.
[Sahai, Nita] Univ Wisconsin, Environm Chem & Technol Program, Madison, WI USA.
RP Sahai, N (reprint author), Univ Akron, Dept Polymer Sci, 170 Univ Ave, Akron, OH 44313 USA.
EM jxu@gwu.edu; sahai@uakron.edu
RI XU, JIE/K-5516-2015
FU NSF [0346689]; NASA Astrobiology Institute Director's Discretionary
Fund; University of Akron; Weeks Graduate Fellowship through the
Department of Geoscience, University of Wisconsin-Madison
FX This research was financially supported by the NSF career award 0346689,
NASA Astrobiology Institute Director's Discretionary Fund 2008 grant,
and by University of Akron "start-up" funds to Nita Sahai. Jie Xu was
supported partially by the Weeks Graduate Fellowship through the
Department of Geoscience, University of Wisconsin-Madison. We thank
Prof. M. Parsek and Prof. Y. Liu for providing the bacterial strains,
Prof. E. Roden for use of the epi-fluores-cence microscope, and Dr. S.
Cheng and Dr. E. Shelobolina for technical assistance and helpful
discussions, which significantly improved the manuscript.
NR 54
TC 5
Z9 5
U1 3
U2 32
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD AUG
PY 2012
VL 12
IS 8
BP 785
EP 798
DI 10.1089/ast.2011.0776
PG 14
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 006IA
UT WOS:000308811500007
PM 22934560
ER
PT J
AU Moncrieff, MW
Waliser, DE
Miller, MJ
Shapiro, MA
Asrar, GR
Caughey, J
AF Moncrieff, Mitchell W.
Waliser, Duane E.
Miller, Martin J.
Shapiro, Melvyn A.
Asrar, Ghassem R.
Caughey, James
TI MULTISCALE CONVECTIVE ORGANIZATION AND THE YOTC VIRTUAL GLOBAL FIELD
CAMPAIGN
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODELS; LARGE-SCALE
ORGANIZATION; CLOUD-RESOLVING MODEL; INCLUDING MASS FLUXES; TROPICAL
CONVECTION; INTRASEASONAL VARIABILITY; MULTICLOUD MODEL; WESTERN
PACIFIC; CLIMATE MODELS
C1 [Moncrieff, Mitchell W.] NCAR, Earth Syst Lab NESL, Climate & Global Dynam Div, Boulder, CO 80305 USA.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Miller, Martin J.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Asrar, Ghassem R.; Caughey, James] World Meteorol Org, Geneva, Switzerland.
RP Moncrieff, MW (reprint author), NCAR, Earth Syst Lab NESL, Climate & Global Dynam Div, 1850 Table Mesa Dr, Boulder, CO 80305 USA.
EM moncrief@ucar.edu
FU NASA through the U.S. THORPEX Executive Committee (USTEC); NOAA through
the U.S. THORPEX Executive Committee (USTEC); NSF through the U.S.
THORPEX Executive Committee (USTEC); National Science Foundation
FX We thank the WWRP/THORPEX and WCRP for their lasting support of the YOTC
project, and NASA, NOAA, and NSF for supporting the YOTC Project Office
through the U.S. THORPEX Executive Committee (USTEC). We thank the ECMWF
for their major commitment to preparing the ECMWF-YOTC database. We
thank Brian Mapes for helpful comments on the manuscript. Duane
Waliser's contribution was carried out on behalf of the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA.; The National Center for Atmospheric Research is sponsored by the
National Science Foundation.
NR 84
TC 52
Z9 53
U1 0
U2 22
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD AUG
PY 2012
VL 93
IS 8
BP 1171
EP 1187
DI 10.1175/BAMS-D-11-00233.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 009WI
UT WOS:000309055700005
ER
PT J
AU Waliser, DE
Moncrieff, MW
Burridge, D
Fink, AH
Gochis, D
Goswami, BN
Guan, B
Harr, P
Heming, J
Hsu, HH
Jakob, C
Janiga, M
Johnson, R
Jones, S
Knippertz, P
Marengo, J
Nguyen, H
Pope, M
Serra, Y
Thorncroft, C
Wheeler, M
Wood, R
Yuter, S
AF Waliser, Duane E.
Moncrieff, Mitchell W.
Burridge, David
Fink, Andreas H.
Gochis, Dave
Goswami, B. N.
Guan, Bin
Harr, Patrick
Heming, Julian
Hsu, Huang-Hsuing
Jakob, Christian
Janiga, Matt
Johnson, Richard
Jones, Sarah
Knippertz, Peter
Marengo, Jose
Hanh Nguyen
Pope, Mick
Serra, Yolande
Thorncroft, Chris
Wheeler, Matthew
Wood, Robert
Yuter, Sandra
TI THE "YEAR" OF TROPICAL CONVECTION (MAY 2008-APRIL 2010) Climate
Variability and Weather Highlights
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; AFRICAN EASTERLY WAVES; NORTH-ATLANTIC
OSCILLATION; GENERAL-CIRCULATION MODEL; SEA-SURFACE TEMPERATURES;
AUSTRALIAN WET SEASON; COUPLED KELVIN WAVES; INDIAN-OCEAN DIPOLE;
LOW-LEVEL JET; SOUTH-AMERICA
C1 [Waliser, Duane E.; Guan, Bin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Moncrieff, Mitchell W.; Gochis, Dave; Goswami, B. N.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Burridge, David] THORPEX, World Meteorol Org, Geneva, Switzerland.
[Fink, Andreas H.] Univ Cologne, Inst Geophys & Meteorol, Cologne, Germany.
[Goswami, B. N.] Indian Inst Trop Meteorol, Pune, Maharashtra, India.
[Harr, Patrick] USN, Postgrad Sch, Monterey, CA USA.
[Heming, Julian] Met Off, Exeter, Devon, England.
[Hsu, Huang-Hsuing] Natl Taiwan Univ, Taipei 10764, Taiwan.
[Jakob, Christian] Monash Univ, Melbourne, Vic 3004, Australia.
[Janiga, Matt; Hanh Nguyen; Thorncroft, Chris] SUNY Albany, Albany, NY 12222 USA.
[Johnson, Richard] Colorado State Univ, Ft Collins, CO 80523 USA.
[Jones, Sarah] Karlsruhe Inst Technol, Karlsruhe, Germany.
[Knippertz, Peter] Univ Leeds, Leeds, W Yorkshire, England.
[Marengo, Jose] Ctr Previsao Tempo & Estudos Climat, Sao Paulo, Brazil.
[Pope, Mick] Bur Meteorol Training Ctr, Bur Meteorol, Melbourne, Vic, Australia.
[Serra, Yolande] Univ Arizona, Tucson, AZ USA.
[Wheeler, Matthew] Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia.
[Wood, Robert] Univ Washington, Seattle, WA 98195 USA.
[Yuter, Sandra] N Carolina State Univ, Raleigh, NC 27695 USA.
RP Waliser, DE (reprint author), CALTECH, Jet Prop Lab, MS 183-505,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM duane.waliser@jpl.nasa.gov
RI Marengo, Jose /J-9382-2012; Wood, Robert/A-2989-2008; Guan,
Bin/F-6735-2010; Jones, Sarah/B-2339-2013; Wheeler, Matthew/C-9038-2011;
Yuter, Sandra/E-8808-2015; Serra, Yolande/I-3457-2015; Knippertz,
Peter/D-5861-2016; Jakob, Christian/A-1082-2010; Fink,
Andreas/F-3024-2017
OI Marengo, Jose /0000-0002-8154-2762; Wood, Robert/0000-0002-1401-3828;
Wheeler, Matthew/0000-0002-9769-1973; Yuter, Sandra/0000-0002-3222-053X;
Serra, Yolande/0000-0003-3542-1158; Knippertz,
Peter/0000-0001-9856-619X; Jakob, Christian/0000-0002-5012-3207; Fink,
Andreas/0000-0002-5840-2120
FU World Climate Research Programme; World Weather Research Programme;
Observing System Research and Prediction Experiment (THORPEX); National
Science Foundation, Mesoscale Dynamic Meteorology Program [ATM-0639461];
National Oceanic and Atmospheric Administration, Office of Global
Programs [NA07OAR4310263]; NOAA's Climate Program Office [NA06OAR43100,
NA08OAR4310705]
FX We would like to express our gratitude to the World Climate Research
Programme, the World Weather Research Programme, and The Observing
System Research and Prediction Experiment (THORPEX) for their joint
support of the YOTC program. This research was supported by the National
Science Foundation, Mesoscale Dynamic Meteorology Program, under Grant
ATM-0639461, and the National Oceanic and Atmospheric Administration,
Office of Global Programs, under Grant NA07OAR4310263. The European
Centre for Medium-Range Weather Forecasts is acknowledged for providing
the special ECMWF YOTC dataset. We thank Paul Ciesielski and Andy Newman
for their assistance in the preparation of figures. The CloudSat and
TRMM data were visualized with the Giovanni online data system,
developed and maintained by the NASA GES DISC. The Meteosat image was
downloaded from the webpage of the Dundee Satellite Receiving Station.
We are grateful to the ECMWF for providing access to the YOTC analysis
and forecast products, and to the French IRD and the National Weather
Services of Benin, Guinea, and Ghana for providing rainfall data for
February 2009. BNG thanks Neena Mani Joseph and Suhas E for their help
in creating the Indian monsoon figures. YLS was supported by NOAA's
Climate Program Office under Grant NA06OAR43100. DJG was supported by
NOAA's Climate Program Office under Grant NA08OAR4310705.
NR 148
TC 77
Z9 77
U1 0
U2 24
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD AUG
PY 2012
VL 93
IS 8
BP 1189
EP 1218
DI 10.1175/2011BAMS3095.1
PG 30
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 009WI
UT WOS:000309055700006
ER
PT J
AU Moncrieff, MW
Waliser, DE
Caughey, J
AF Moncrieff, Mitchell W.
Waliser, Duane E.
Caughey, James
TI PROGRESS AND DIRECTION IN TROPICAL CONVECTION RESEARCH YOTC
International Science Symposium
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
C1 [Moncrieff, Mitchell W.] NCAR, Climate & Global Dynam Div, Boulder, CO 80305 USA.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Caughey, James] WMO, THORPEX Int Programme Off, Geneva, Switzerland.
RP Moncrieff, MW (reprint author), NCAR, Climate & Global Dynam Div, 1850 Table Mesa Dr, Boulder, CO 80305 USA.
EM moncrief@ucar.edu
NR 2
TC 3
Z9 3
U1 1
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD AUG
PY 2012
VL 93
IS 8
BP ES65
EP ES69
DI 10.1175/BAMS-D-11-00253.1
PG 5
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 009WI
UT WOS:000309055700001
ER
PT J
AU Zhang, P
Imhoff, ML
Bounoua, L
Wolfe, RE
AF Zhang, Ping
Imhoff, Marc L.
Bounoua, Lahouari
Wolfe, Robert E.
TI Exploring the influence of impervious surface density and shape on urban
heat islands in the northeast United States using MODIS and Landsat
SO CANADIAN JOURNAL OF REMOTE SENSING
LA English
DT Article
ID TEMPERATURE; CITY; PRODUCTS; CLIMATE; INDEXES; URBANIZATION; VALIDATION;
SIMULATION; GROWTH; AREA
AB Impervious surface area (ISA) from the National Land Cover Database 2001 and land surface skin temperature from MODIS averaged over three annual cycles (2003-2005) are used in a spatial analysis to assess the surface urban heat island (UHI) signature and its relationship to settlement size and shape, development intensity distribution, and land cover composition for 42 urban settlements embedded in forest biomes in the northeastern United States. Development intensity zones, based on percent ISA, are defined for each urban area emanating outward from the urban core to nearby rural areas and are used to stratify land surface temperature. The stratification is further constrained by biome type and elevation to ensure objective intercomparisons between urban zones within an urban settlement and between settlements. Stratification based on ISA allows the definition of hierarchically ordered urban zones that are consistent across urban settlements and scales. For cities within the northeastern US temperate mixed forest biome, we found that settlement size, shape, and development intensity significantly influenced the amplitude of summer daytime UHI. Our study indicates that for cities of similar size, the ISA density distribution within the urban area and the shape of the urbanized area as measured by area to perimeter ratio are significant modulators of UHI magnitude. Our results indicate that remotely sensed satellite data provide a consistent characterization of the UHI magnitude as well as its major drivers across regional scales.
C1 [Zhang, Ping; Imhoff, Marc L.; Bounoua, Lahouari; Wolfe, Robert E.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Zhang, Ping] Earth Resource Technol Inc, Laurel, MD 20707 USA.
RP Zhang, P (reprint author), NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
EM Ping.zhang-1@nasa.gov
RI Wolfe, Robert/E-1485-2012
OI Wolfe, Robert/0000-0002-0915-1855
NR 39
TC 11
Z9 11
U1 0
U2 34
PU CANADIAN AERONAUTICS & SPACE INST
PI KANATA
PA 350 TERRY FOX DR, STE 104, KANATA, ON K2K 2W5, CANADA
SN 0703-8992
EI 1712-7971
J9 CAN J REMOTE SENS
JI Can. J. Remote Sens.
PD AUG
PY 2012
VL 38
IS 4
BP 441
EP 451
PG 11
WC Remote Sensing
SC Remote Sensing
GA 010PK
UT WOS:000309106400002
ER
PT J
AU Truong-Loi, ML
Dubois-Fernandez, P
Pottier, E
AF Truong-Loi, M-L.
Dubois-Fernandez, P.
Pottier, E.
TI Assessment of forest biomass retrieval from compact-pol SAR data
SO CANADIAN JOURNAL OF REMOTE SENSING
LA English
DT Article
ID RADAR BACKSCATTER
AB In this paper, the potential of compact polarimetric data at low frequency for aboveground biomass retrieval is explored on an extensively studied maritime pine plantation forest situated on flat topography. Aboveground biomass was calculated at 55 stands using site-specific allometric equations. The site biomass level is up to 120 t/ha with a mean observed biomass of 66.7 t/ha. The P-band synthetic aperture radar (SAR) dataset acquired by the Office National d'Etudes et de Recherches Aerospatiales' airborne SAR system, known as RAMSES, is fully polarimetric and can be used to compute the compact polarimetric data associated with a circularly polarized transmit polarization and two mutually coherent independent polarizations. Information acquired with a compact polarimetric (CP) system is reduced compared with full polarimetry (FP) (i.e., the information in CP is represented by a two-dimensional complex vector resulting in four parameters; whereas, in FP, considering a monostatic case, the representation requires a three-dimensional complex vector with six independent parameters). The linear cross-polarized channel horizontal-vertical (HV) has been shown to be of significant relevance for forestry studies but is not directly measured in the standard CP modes. The challenge of this CP study was then to find alternate indicators specific to CP allowing accurate biomass retrieval. Such indicators are proposed for the compact mode for which the transmit polarization is circularly polarized and their sensitivity to biomass are quantified through a correlation analysis. The corresponding coefficients of determination are observed to be of the order of 0.9 comparable with the number obtained for FP data. Various estimation algorithms based on the regression curves were proposed and evaluated on the 55 test stands. The results obtained with CP data agree quite closely with those obtained with FP data with a measured accuracy in root mean square error within 6 t/ha. This shows that for biomass estimation, in the case of a flat topography, CP can be used instead of HV making it an interesting mode of operation for future spaceborne SAR such as the European BIOMASS mission.
C1 [Truong-Loi, M-L.; Dubois-Fernandez, P.] Off Natl Etud & Rech Aerosp, BA 701, F-13661 Salon Air, France.
[Pottier, E.] CNRS, IETR, UMR 6164, CS 74205, F-35042 Rennes, France.
RP Truong-Loi, ML (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, La Canada Flintridge, CA 91011 USA.
EM my-linh.truong-loi@jpl.nasa.gov
RI Dubois-Fernandez, Pascale/A-6743-2012
FU CNES; ONERA
FX The authors would like to thank their colleagues from the
Electromagnetism and Radar Department (DEMR/RIM) of the French Aerospace
Lab (ONERA) for providing the RAMSES data and Isabelle Champion, Ephyse,
INRA for providing the in situ measurements. The research was conducted
under a grant by CNES and ONERA.
NR 17
TC 4
Z9 4
U1 1
U2 7
PU CANADIAN AERONAUTICS SPACE INST
PI KANATA
PA 350 TERRY FOX DR, STE 104, KANATA, ON K2K 2W5, CANADA
SN 1712-7971
J9 CAN J REMOTE SENS
JI Can. J. Remote Sens.
PD AUG
PY 2012
VL 38
IS 4
BP 452
EP 460
PG 9
WC Remote Sensing
SC Remote Sensing
GA 010PK
UT WOS:000309106400003
ER
PT J
AU Aggarwal, JK
Ryoo, MS
AF Aggarwal, J. K.
Ryoo, M. S.
TI Toward a unified framework of motion understanding
SO IMAGE AND VISION COMPUTING
LA English
DT Article
DE Opinion paper; Motion understanding; Human activity recognition
C1 [Aggarwal, J. K.] Univ Texas Austin, Comp & Vis Res Ctr, Austin, TX 78712 USA.
[Ryoo, M. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Aggarwal, JK (reprint author), Univ Texas Austin, Comp & Vis Res Ctr, Austin, TX 78712 USA.
EM aggarwaljk@mail.utexas.edu; mryoo@jpl.nasa.jov
NR 12
TC 0
Z9 0
U1 0
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0262-8856
J9 IMAGE VISION COMPUT
JI Image Vis. Comput.
PD AUG
PY 2012
VL 30
IS 8
BP 465
EP 466
DI 10.1016/j.imavis.2011.12.012
PG 2
WC Computer Science, Artificial Intelligence; Computer Science, Software
Engineering; Computer Science, Theory & Methods; Engineering, Electrical
& Electronic; Optics
SC Computer Science; Engineering; Optics
GA 007QV
UT WOS:000308904100002
ER
PT J
AU Leroy, SS
Ao, CO
Verkhoglyadova, O
AF Leroy, Stephen S.
Ao, Chi O.
Verkhoglyadova, Olga
TI Mapping GPS Radio Occultation Data by Bayesian Interpolation
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID GLOBAL POSITIONING SYSTEM; ERA-INTERIM REANALYSIS; ASSIMILATION;
ATMOSPHERE; MISSION
AB Bayesian interpolation for mapping GPS radio occultation data on a sphere is explored and its performance evaluated. Bayesian interpolation is ideally suited to the task of fitting data randomly and nonuniformly distributed with unknown error without overfitting the data. The geopotential height at dry pressure 200 hPa is simulated as data with theoretical distributions of the Challenging Mini-Satellite Payload (CHAMP) and of the Constellation Observing System for Meteorology, Ionosphere and Climate (COSMIC). The simulated CHAMP data are found to be best fit with a spherical harmonic basis of 14th degree; the COSMIC data with a spherical harmonic basis of 20th degree. The best regularizer mimics a spline fit, and relaxing the penalty for purely meridional structures or for the global mean yields little advantage. Climatologies are most accurately established by binning in similar or equal to 2-days intervals to best resolve synoptic structures in space and time. Finally, Bayesian interpolation is shown to negate a source of systematic sampling error obtained in binning and averaging highly nonuniform data but to incur another systematic error due to incomplete resolution of the background atmosphere, notably in the Southern Hemisphere.
C1 [Leroy, Stephen S.] Harvard Univ, Harvard Sch Engn & Appl Sci, Anderson Grp, Cambridge, MA 02138 USA.
[Ao, Chi O.; Verkhoglyadova, Olga] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Leroy, SS (reprint author), Harvard Univ, Harvard Sch Engn & Appl Sci, Anderson Grp, 12 Oxford St,Link Bldg, Cambridge, MA 02138 USA.
EM leroy@huarp.harvard.edu
RI Richards, Amber/K-8203-2015;
OI Verkhoglyadova, Olga/0000-0002-9295-9539
FU NASA [NNX11AD01G]; NASA Jet Propulsion Laboratory's Director's Research
and Development Fund
FX This work was supported in part by NASA Grant NNX11AD01G and by a grant
from the NASA Jet Propulsion Laboratory's Director's Research and
Development Fund. Work performed by C. Ao and O. Verkhoglyadova was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 22
TC 4
Z9 4
U1 0
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD AUG
PY 2012
VL 29
IS 8
BP 1062
EP 1074
DI 10.1175/JTECH-D-11-00179.1
PG 13
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 994BQ
UT WOS:000307906300006
ER
PT J
AU Wang, XC
Chao, Y
Shum, CK
Yi, YC
Fok, HS
AF Wang, Xiaochun
Chao, Yi
Shum, C. K.
Yi, Yuchan
Fok, Hok Sum
TI Comparison of Two Methods to Assess Ocean Tide Models
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID TOPEX/POSEIDON; ALTIMETRY
AB Two methods to assess ocean tide models, the current method and the total discrepancy method, are compared from the perspective of their relationship to the root-mean-square difference of tidal sea surface height (total discrepancy). These two methods are identically the same when there is only one spatial location involved. When there is more than one spatial location involved, the current method is the root-mean-square difference of total discrepancy at each location, and the total discrepancy method is the averaged total discrepancy. The result from the current method is always larger than or equal to that from the total discrepancy method. Monte Carlo simulation indicates that the difference between their results increases with increasing spatial variability of total discrepancy. Both of these two methods are then used to compare the two tide models of the Ocean Surface Topography Mission (OSTM)/Jason-2. The discrepancy of these two models as measured by the total discrepancy method decreases monotonically from around 11.4 to 2.2 cm with depth increasing from 50 to 1000 m. In contrast, the discrepancy measured by the current method varies from 21.6 to 2.9 cm. Though the discrepancy measured by the current method decreases with increasing depth in general, there are abrupt increases at several depth ranges. These increases are associated with large spatial variability of total discrepancy and their physical explanation is elusive. Because the total discrepancy method is consistent with the root-mean-square difference of tidal sea surface height and its interpretation is straightforward, its usage is suggested.
C1 [Wang, Xiaochun] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90095 USA.
[Chao, Yi] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Shum, C. K.; Yi, Yuchan; Fok, Hok Sum] Ohio State Univ, Sch Earth Sci, Div Geodet Sci, Columbus, OH 43210 USA.
RP Wang, XC (reprint author), Univ Calif Los Angeles, JIFRESSE, Box 957228,9258 Boelter Hall, Los Angeles, CA 90095 USA.
EM xcwang@jifresse.ucla.edu
FU Jet Propulsion Laboratory (JPL); NASA's Physical Oceanography Program
under the Ocean Surface Topography Science Team (OSTST); California
Institute of Technology; National Aeronautics and Space Administration
FX The research was carried out, in part, by the Jet Propulsion Laboratory
(JPL), California Institute of Technology, under contract with the
National Aeronautics and Space Administration. The Ohio State University
component of this research is supported by grants from NASA's Physical
Oceanography Program under the Ocean Surface Topography Science Team
(OSTST). Dr. F. Lefevre provided the FES2004 tidal solution and Dr. R.
Ray provided the GOT00 tidal solution. The insightful comments from two
anonymous reviewers helped us greatly during the revision process.
NR 12
TC 1
Z9 1
U1 1
U2 4
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD AUG
PY 2012
VL 29
IS 8
BP 1159
EP 1167
DI 10.1175/JTECH-D-11-00166.1
PG 9
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 994BQ
UT WOS:000307906300014
ER
PT J
AU Wu, H
Adler, RF
Hong, Y
Tian, YD
Policelli, F
AF Wu, Huan
Adler, Robert F.
Hong, Yang
Tian, Yudong
Policelli, Fritz
TI Evaluation of Global Flood Detection Using Satellite-Based Rainfall and
a Hydrologic Model
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID PRECIPITATION ANALYSIS TMPA; RIVER-BASIN; INFORMATION; SYSTEMS; STORAGE;
RUNOFF
AB A new version of a real-time global flood monitoring system (GFMS) driven by Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA) rainfall has been developed and implemented using a physically based hydrologic model. The purpose of this paper is to evaluate the performance of this new version of the GFMS in terms of flood event detection against flood event archives to establish a baseline of performance and directions for improvement. This new GFMS is quantitatively evaluated in terms of flood event detection during the TRMM era (1998-2010) using a global retrospective simulation (3-hourly and 1/8 degrees spatial resolution) with the TMPA 3B42V6 rainfall. Four methods were explored to define flood thresholds from the model results, including three percentile-based statistical methods and a Log Pearson type-Ill flood frequency curve method. The evaluation showed the GFMS detection performance improves [increasing probability of detection (POD)] with longer flood durations and larger affected areas. The impact of dams was detected in the validation statistics, with the presence of dams tending to result in more false alarms and greater false-alarm duration. The GFMS validation statistics for flood durations >3 days and for areas without dams vary across the four methods, but center around a POD of similar to 0.70 and a false-alarm rate (FAR) of similar to 0.65. The generally positive results indicate the value of this approach for monitoring and researching floods on a global scale, but also indicate limitations and directions for improvement of such approaches. These directions include improving the rainfall estimates, utilizing higher resolution in the runoff-routing model, taking into account the presence of dams, and improving the method for flood identification.
C1 [Wu, Huan; Adler, Robert F.; Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Wu, Huan; Adler, Robert F.; Tian, Yudong; Policelli, Fritz] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hong, Yang] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
[Hong, Yang] Univ Oklahoma, Atmospher Radar Res Ctr, Norman, OK 73019 USA.
RP Wu, H (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, 5825 Univ Court,Suite 4001, College Pk, MD 20740 USA.
EM huanwu@umd.edu
RI Hong, Yang/D-5132-2009; Wu, Huan/K-1003-2013; Measurement,
Global/C-4698-2015
OI Hong, Yang/0000-0001-8720-242X; Wu, Huan/0000-0003-2920-8860;
FU NASA's Applied Sciences Program; NASA's Precipitation Measurement
Missions (PMM) Program
FX This work was supported by NASA's Applied Sciences Program (Michael
Goodman) and NASA's Precipitation Measurement Missions (PMM) Program
(Ramesh Kakar).
NR 35
TC 49
Z9 50
U1 3
U2 23
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD AUG
PY 2012
VL 13
IS 4
BP 1268
EP 1284
DI 10.1175/JHM-D-11-087.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 994BS
UT WOS:000307906500007
ER
PT J
AU Kirstetter, PE
Hong, Y
Gourley, JJ
Chen, S
Flamig, Z
Zhang, J
Schwaller, M
Petersen, W
Amitai, E
AF Kirstetter, Pierre-Emmanuel
Hong, Y.
Gourley, J. J.
Chen, S.
Flamig, Z.
Zhang, J.
Schwaller, M.
Petersen, W.
Amitai, E.
TI Toward a Framework for Systematic Error Modeling of Spaceborne
Precipitation Radar with NOAA/NSSL Ground Radar Based National Mosaic
QPE
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID RAINFALL ESTIMATION; SATELLITE; VALIDATION; AFRICA
AB Characterization of the error associated with satellite rainfall estimates is a necessary component of deterministic and probabilistic frameworks involving spaceborne passive and active microwave measurements for applications ranging from water budget studies to forecasting natural hazards related to extreme rainfall events. The authors focus here on the error structure of NASA's Tropical Rainfall Measurement Mission (TRMM) Precipitation Radar (PR) quantitative precipitation estimation (QPE) at ground. The problem is addressed by comparison of PR QPEs with reference values derived from ground-based measurements using NOAA/NSSL ground radar based National Mosaic and QPE system (NMQ/Q2). A preliminary investigation of this subject has been carried out at the PR estimation scale (instantaneous and 5 km) using a 3-month data sample in the southern part of the United States. The primary contribution of this study is the presentation of the detailed steps required to derive a trustworthy reference rainfall dataset from Q2 at the PR pixel resolution. It relies on a bias correction and a radar quality index, both of which provide a basis to filter out the less trustworthy Q2 values. Several aspects of PR errors are revealed and quantified including sensitivity to the processing steps with the reference rainfall, comparisons of rainfall delectability and rainfall-rate distributions, spatial representativeness of error, and separation of systematic biases and random errors. The methodology and framework developed herein applies more generally to rainfall-rate estimates from other sensors on board low-earth-orbiting satellites such as microwave imagers and dual-wavelength radars such as with the Global Precipitation Measurement (GPM) mission.
C1 [Kirstetter, Pierre-Emmanuel; Hong, Y.; Chen, S.] Natl Weather Ctr, Atmospher Radar Res Ctr, Norman, OK 73072 USA.
[Kirstetter, Pierre-Emmanuel; Hong, Y.; Chen, S.] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
[Kirstetter, Pierre-Emmanuel; Gourley, J. J.; Flamig, Z.; Zhang, J.] NOAA, Natl Severe Storms Lab, Norman, OK USA.
[Flamig, Z.] Cooperat Inst Mesoscale Meteorol Studies, Norman, OK USA.
[Schwaller, M.; Amitai, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Petersen, W.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
[Amitai, E.] Chapman Univ, Orange, CA USA.
RP Hong, Y (reprint author), Natl Weather Ctr, Atmospher Radar Res Ctr, 120 David L Boren Blvd,Rm 4610, Norman, OK 73072 USA.
EM yanghong@ou.edu
RI Hong, Yang/D-5132-2009; Kirstetter, Pierre/E-2305-2013; Measurement,
Global/C-4698-2015; Gourley, Jonathan/C-7929-2016
OI Hong, Yang/0000-0001-8720-242X; Kirstetter, Pierre/0000-0002-7381-0229;
Gourley, Jonathan/0000-0001-7363-3755
FU NASA Global Precipitation Measurement Mission Ground Validation
Management
FX We are very much indebted to the team responsible for the NMQ/Q2
products, especially Carrie Langston. We want to thank two anonymous
reviewers whose comments were very useful for improving the manuscript.
This work was funded by a postdoctoral grant from the NASA Global
Precipitation Measurement Mission Ground Validation Management.
NR 36
TC 36
Z9 36
U1 1
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD AUG
PY 2012
VL 13
IS 4
BP 1285
EP 1300
DI 10.1175/JHM-D-11-0139.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 994BS
UT WOS:000307906500008
ER
PT J
AU Murray, JA
Benyahia, S
Metzger, P
Hrenya, CM
AF Murray, J. A.
Benyahia, S.
Metzger, P.
Hrenya, C. M.
TI Continuum representation of a continuous size distribution of particles
engaged in rapid granular flow
SO PHYSICS OF FLUIDS
LA English
DT Article
ID KINETIC-THEORY APPROACH; FLUIDIZED-BEDS; GAS/PARTICLE FLOW; SEGREGATION;
MIXTURES; MODEL
AB Natural and industrial granular flows often consist of several particle sizes, approximately forming a continuous particle size distribution (PSD). Continuous PSDs are ubiquitous, though existing kinetic-theory-based, hydrodynamic models for rapid granular flows are limited to a discrete number of species. The objective of this work is twofold: (i) to determine the number of discrete species required to accurately approximate a continuous PSD and (ii) to validate these results via a comparison with molecular dynamics (MD) simulations of continuous PSDs. With regard to the former, several analytic (Gaussian and lognormal) and experimental (coal and lunar soil simulants) distributions are investigated. Transport coefficients (pressure, shear viscosity, etc.) of the granular mixture given by the polydisperse theory of Garzo et al. ["Enskog theory for polydisperse granular mixtures. I. Navier-Stokes order transport," Phys. Rev. E 76, 031303 (2007); "Enskog theory for polydisperse granular mixtures. I. Navier-Stokes order transport," 76, 031304 (2007)] are compared using an increasing number of species s to approximate the given PSD. These discrete approximations are determined by matching the first 2s moments of the approximation and the given continuous distribution. Relatively few species are required to approximate moderately wide distributions (Gaussian, lognormal), whereas even wider distributions (coal and lunar soil simulants) require a larger number of species. Regarding the second objective, a comparison between MD simulations and kinetic-theory predictions for a simple shear flow of both Gaussian and lognormal PSDs reveal essentially no loss of accuracy stemming from the polydisperse theory itself (as compared to theories for monodisperse systems) or from the discrete approximations of continuous PSDs used in the polydisperse theory. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4744987]
C1 [Murray, J. A.; Hrenya, C. M.] Univ Colorado, Dept Chem & Biol Engn, Boulder, CO 80309 USA.
[Benyahia, S.] Natl Energy Technol Lab, Morgantown, WV 26507 USA.
[Metzger, P.] NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA.
RP Hrenya, CM (reprint author), Univ Colorado, Dept Chem & Biol Engn, Boulder, CO 80309 USA.
EM hrenya@colorado.edu
RI Metzger, Philip/R-3136-2016
OI Metzger, Philip/0000-0002-6871-5358
FU Department of Energy [DE-FC26-07NT43098]; National Aeronautics and Space
Administration [NNX09AD07A]
FX The authors would like to thank Larry Shadle of the (U.S.) Department of
Energy (DOE) NETL for providing the bidisperse gasifier data, Rodney Fox
for providing code to obtain the discrete approximations, and Vicente
Garzo for fruitful discussions. Also, we are grateful for the funding
support by the Department of Energy (DE-FC26-07NT43098) and the National
Aeronautics and Space Administration (NNX09AD07A).
NR 25
TC 3
Z9 3
U1 1
U2 21
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-6631
EI 1089-7666
J9 PHYS FLUIDS
JI Phys. Fluids
PD AUG
PY 2012
VL 24
IS 8
AR 083303
DI 10.1063/1.4744987
PG 19
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 000VD
UT WOS:000308417000026
ER
PT J
AU Erzberger, H
Lauderdale, TA
Chu, YC
AF Erzberger, H.
Lauderdale, T. A.
Chu, Y-C
TI Automated conflict resolution, arrival management, and weather avoidance
for air traffic management
SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF
AEROSPACE ENGINEERING
LA English
DT Article
DE separation assurance; air traffic management
AB This article describes a unified solution to three types of separation-assurance problems that occur in en-route airspace: separation conflicts, arrival sequencing, and weather-cell avoidance. Algorithms for solving these problems play a key role in the design of future air traffic management systems such as the US's NextGen. Because these problems can arise simultaneously in any combination, it is necessary to develop integrated algorithms for solving them. A unified and comprehensive solution to these problems provides the foundation for a future air traffic management system that requires a high level of automation in separation assurance. This article describes the three algorithms developed for solving each problem and then shows how they are used sequentially to solve any combination of these problems. The first set of algorithms resolves loss-of-separation conflicts. It generates multiple resolutions for each conflict and then selects the one giving the least delay. Two new algorithms, one for sequencing and merging of arrival traffic, referred to as the arrival manager, and the other for weather-cell avoidance are presented. Because these three problems constitute a substantial fraction of the workload of en-route controllers, integrated algorithms to solve them is a basic requirement for automated separation assurance. This article also reviews the advanced airspace concept, a proposed design for a ground-based system that postulates redundant systems for automated separation assurance in order to achieve both high levels of safety and airspace capacity. It is proposed that automated separation assurance be introduced operationally in several steps, each step reducing controller workload further while increasing airspace capacity. A fast time simulation was used to determine performance statistics of the algorithm at up to 3x current traffic levels.
C1 [Erzberger, H.; Chu, Y-C] NASA, Ames Res Ctr, Aerosp Comp Inc, Moffett Field, CA 94035 USA.
[Erzberger, H.] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA.
RP Erzberger, H (reprint author), NASA, Ames Res Ctr, Aerosp Comp Inc, Mail Stop 210-10,Bldg N210,Room 230,POB 1, Moffett Field, CA 94035 USA.
EM Heinz.Erzberger@nasa.gov
NR 15
TC 2
Z9 2
U1 0
U2 9
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0954-4100
J9 P I MECH ENG G-J AER
JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng.
PD AUG
PY 2012
VL 226
IS G8
BP 930
EP 949
DI 10.1177/0954410011417347
PG 20
WC Engineering, Aerospace; Engineering, Mechanical
SC Engineering
GA 992GB
UT WOS:000307762500004
ER
EF