FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Stefanik, RP
Torres, G
Latham, DW
Landsman, W
Craig, N
Murrett, J
AF Stefanik, Robert P.
Torres, Guillermo
Latham, David W.
Landsman, Wayne
Craig, Nathaniel
Murrett, James
TI OBSERVATIONS AND ORBITAL ANALYSIS OF THE GIANT WHITE DWARF BINARY SYSTEM
HR 5692
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: general; methods: data analysis; stars: individual (HR 5692);
techniques: spectroscopic; white dwarfs
ID INTERMEDIATE ASTROMETRIC DATA; RADIAL-VELOCITIES; SPECTROSCOPIC
BINARIES; BARIUM STARS; S STARS; MASS; CATALOG; EXTINCTION; ISOCHRONES;
SIRIUS
AB We report spectroscopic observations of the red giant star HR5692, previously known to be a binary system both from other spectroscopic work and from deviations in the astrometric motion detected by the Hipparcos satellite. Earlier International Ultraviolet Explorer (IUE) observations had shown the presence of a hot white dwarf companion to the giant primary. We have combined our radial velocity observations with other existing measurements and with the Hipparcos intermediate astrometric data to determine a complete astrometric-spectroscopic orbital solution, providing the inclination angle for the first time. We also determine an improved parallax for the system of 10.12 +/- 0.67 mas. We derive the physical properties of the primary, and with an estimate of its mass from stellar evolution models (1.84 +/- 0.40M(circle dot)), we infer the mass of the white dwarf companion to be M-WD = 0.59 +/- 0.12M(circle dot). An analysis of an IUE white dwarf spectrum, using our parallax, yields T-eff = 30,400 +/- 780 K, log g = 8.25 +/- 0.15, and a mass M-WD = 0.79 +/- 0.09M(circle dot), in marginal agreement with the dynamical mass.
C1 [Stefanik, Robert P.; Torres, Guillermo; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Landsman, Wayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Craig, Nathaniel; Murrett, James] Harvard Univ, Cambridge, MA 02138 USA.
RP Stefanik, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rstefanik@cfa.harvard.edu
FU NSF [AST-0708229, AST-1007992]; NASA [NAS5-26555]; NASA Office of Space
Science [NNX09AF08G]
FX We thank Michael Calkins, Joe Caruso, Gil Esquerdo, and Joe Zajac for
obtaining many of the spectroscopic observations used here. We also
thank I. Hubeny for his assistance with the TLUSTY code. G. T.
acknowledges partial support for this work from NSF grants AST-0708229
and AST-1007992. This research has made use of the SIMBAD database and
the VizieR catalog access tool, both operated at CDS, Strasbourg,
France, of NASA's Astrophysics Data System Abstract Service, and of data
products from the Two Micron All Sky Survey (2MASS), which is a joint
project of the University of Massachusetts and the Infrared Processing
and Analysis Center/California Institute of Technology, funded by NASA
and the NSF. Some 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 NNX09AF08G and by other grants and contracts.
NR 56
TC 4
Z9 4
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2011
VL 141
IS 5
AR 144
DI 10.1088/0004-6256/141/5/144
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 746JB
UT WOS:000289240800003
ER
PT J
AU Batista, V
Gould, A
Dieters, S
Dong, S
Bond, I
Beaulieu, JP
Maoz, D
Monard, B
Christie, GW
McCormick, J
Albrow, MD
Horne, K
Tsapras, Y
Burgdorf, MJ
Novati, SC
Skottfelt, J
Caldwell, J
Kozlowski, S
Kubas, D
Gaudi, BS
Han, C
Bennett, DP
An, J
Abe, F
Botzler, CS
Douchin, D
Freeman, M
Fukui, A
Furusawa, K
Hearnshaw, JB
Hosaka, S
Itow, Y
Kamiya, K
Kilmartin, PM
Korpela, A
Lin, W
Ling, CH
Makita, S
Masuda, K
Matsubara, Y
Miyake, N
Muraki, Y
Nagaya, M
Nishimoto, K
Ohnishi, K
Okumura, T
Perrott, YC
Rattenbury, N
Saito, T
Sullivan, DJ
Sumi, T
Sweatman, WL
Tristram, PJ
Von Seggern, E
Yock, PCM
Brillant, S
Calitz, JJ
Cassan, A
Cole, A
Cook, K
Coutures, C
Prester, DD
Donatowicz, J
Greenhill, J
Hoffman, M
Jablonski, F
Kane, SR
Kains, N
Marquette, JB
Martin, R
Martioli, E
Meintjes, P
Menzies, J
Pedretti, E
Pollard, K
Sahu, KC
Vinter, C
Wambsganss, J
Watson, R
Williams, A
Zub, M
Allen, W
Bolt, G
Bos, M
Depoy, DL
Drummond, J
Eastman, JD
Gal-Yam, A
Gorbikov, E
Higgins, D
Janczak, J
Kaspi, S
Lee, CU
Mallia, F
Maury, A
Monard, LAG
Moorhouse, D
Morgan, N
Natusch, T
Ofek, EO
Park, BG
Pogge, RW
Polishook, D
Santallo, R
Shporer, A
Spector, O
Thornley, G
Yee, JC
Bozza, V
Browne, P
Dominik, M
Dreizler, S
Finet, F
Glitrup, M
Grundahl, F
Harpsoe, K
Hessman, FV
Hinse, TC
Hundertmark, M
Jorgensen, UG
Liebig, C
Maier, G
Mancini, L
Mathiasen, M
Rahvar, S
Ricci, D
Scarpetta, G
Southworth, J
Surdej, J
Zimmer, F
Allan, A
Bramich, DM
Snodgrass, C
Steele, IA
Street, RA
AF Batista, V.
Gould, A.
Dieters, S.
Dong, S.
Bond, I.
Beaulieu, J. P.
Maoz, D.
Monard, B.
Christie, G. W.
McCormick, J.
Albrow, M. D.
Horne, K.
Tsapras, Y.
Burgdorf, M. J.
Novati, S. Calchi
Skottfelt, J.
Caldwell, J.
Kozlowski, S.
Kubas, D.
Gaudi, B. S.
Han, C.
Bennett, D. P.
An, J.
Abe, F.
Botzler, C. S.
Douchin, D.
Freeman, M.
Fukui, A.
Furusawa, K.
Hearnshaw, J. B.
Hosaka, S.
Itow, Y.
Kamiya, K.
Kilmartin, P. M.
Korpela, A.
Lin, W.
Ling, C. H.
Makita, S.
Masuda, K.
Matsubara, Y.
Miyake, N.
Muraki, Y.
Nagaya, M.
Nishimoto, K.
Ohnishi, K.
Okumura, T.
Perrott, Y. C.
Rattenbury, N.
Saito, To.
Sullivan, D. J.
Sumi, T.
Sweatman, W. L.
Tristram, P. J.
Von Seggern, E.
Yock, P. C. M.
Brillant, S.
Calitz, J. J.
Cassan, A.
Cole, A.
Cook, K.
Coutures, C.
Prester, D. Dominis
Donatowicz, J.
Greenhill, J.
Hoffman, M.
Jablonski, F.
Kane, S. R.
Kains, N.
Marquette, J. -B.
Martin, R.
Martioli, E.
Meintjes, P.
Menzies, J.
Pedretti, E.
Pollard, K.
Sahu, K. C.
Vinter, C.
Wambsganss, J.
Watson, R.
Williams, A.
Zub, M.
Allen, W.
Bolt, G.
Bos, M.
Depoy, D. L.
Drummond, J.
Eastman, J. D.
Gal-Yam, A.
Gorbikov, E.
Higgins, D.
Janczak, J.
Kaspi, S.
Lee, C. -U.
Mallia, F.
Maury, A.
Monard, L. A. G.
Moorhouse, D.
Morgan, N.
Natusch, T.
Ofek, E. O.
Park, B. -G.
Pogge, R. W.
Polishook, D.
Santallo, R.
Shporer, A.
Spector, O.
Thornley, G.
Yee, J. C.
Bozza, V.
Browne, P.
Dominik, M.
Dreizler, S.
Finet, F.
Glitrup, M.
Grundahl, F.
Harpsoe, K.
Hessman, F. V.
Hinse, T. C.
Hundertmark, M.
Jorgensen, U. G.
Liebig, C.
Maier, G.
Mancini, L.
Mathiasen, M.
Rahvar, S.
Ricci, D.
Scarpetta, G.
Southworth, J.
Surdej, J.
Zimmer, F.
Allan, A.
Bramich, D. M.
Snodgrass, C.
Steele, I. A.
Street, R. A.
CA MOA Collaboration
PLANET Collaboration
FUN Collaboration
MiNDSTEp Consortium
RoboNet Collaboration
TI MOA-2009-BLG-387Lb: a massive planet orbiting an M dwarf
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: micro; methods: data analysis; planets and
satellites: detection; methods: numerical; instrumentation: adaptive
optics; instrumentation: photometers
ID GALACTIC BULGE; MICROLENSING EVENT; JUPITER/SATURN ANALOG; GIANT
PLANETS; SNOW LINE; STARS; MASSES; PHOTOMETRY; COOL; LUMINOSITY
AB Aims. We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M-circle dot < M-host < 0.49 M-circle dot at 90% confidence. The planet-star mass ratio q = 0.0132 +/- 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is m(p) = 2.6 Jupiter masses for the median host mass, M = 0.19 M-circle dot.
Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius theta(E) = 0.31 +/- 0.03 mas has been accurately measured, but the other (the microlens parallax pi(E), which is due to the Earth's orbital motion) is highly degenerate with the orbital motion of the planet. We statistically resolve the degeneracy between Earth and planet orbital effects by imposing priors from a Galactic model that specifies the positions and velocities of lenses and sources and a Kepler model of orbits.
Results. The 90% confidence intervals for the distance, semi-major axis, and period of the planet are 3.5 kpc < D-L < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively.
C1 [Batista, V.; Dieters, S.; Beaulieu, J. P.; Albrow, M. D.; Horne, K.; Tsapras, Y.; Caldwell, J.; Kubas, D.; Bennett, D. P.; Bramich, D. M.] Probing Lensing Anomalies NETwork PLANET, Chicago, IL USA.
[Dieters, S.; Beaulieu, J. P.; Kubas, D.; Cassan, A.; Marquette, J. -B.] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, F-75014 Paris, France.
[Gould, A.; Dong, S.; Maoz, D.; Monard, B.; Christie, G. W.; McCormick, J.; Gaudi, B. S.; Han, C.] Microlensing Follow Network FUN, New York, NY USA.
[Gould, A.; Kozlowski, S.; Gaudi, B. S.; Eastman, J. D.; Janczak, J.; Morgan, N.; Pogge, R. W.; Yee, J. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Dong, S.] Inst Adv Study, Princeton, NJ 08540 USA.
[Bond, I.; Bennett, D. P.] MOA, Notre Dame, IN USA.
[Bond, I.; Lin, W.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, N Shore Mail Ctr, Auckland, New Zealand.
[Maoz, D.; Gorbikov, E.; Kaspi, S.; Polishook, D.; Shporer, A.; Spector, O.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Maoz, D.; Gorbikov, E.; Kaspi, S.; Polishook, D.; Shporer, A.; Spector, O.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel.
[Monard, B.; Monard, L. A. G.] Ctr Backyard Astrophys, Bronberg Observ, Pretoria, South Africa.
[Christie, G. W.] Auckland Observ, Auckland, New Zealand.
[McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand.
[Albrow, M. D.; Hearnshaw, J. B.; Pollard, K.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Horne, K.; Tsapras, Y.; Rattenbury, N.; Kains, N.] RoboNet Collaborat, Chicago, IL USA.
[Horne, K.; Kains, N.; Pedretti, E.; Browne, P.; Dominik, M.; Liebig, C.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Burgdorf, M. J.; Novati, S. Calchi; Skottfelt, J.; Wambsganss, J.; Snodgrass, C.] Microlensing Network Detect Small Terr Exoplanets, Les Ulis, France.
[Skottfelt, J.; Vinter, C.; Harpsoe, K.; Hinse, T. C.; Jorgensen, U. G.; Mathiasen, M.; Zimmer, F.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Jorgensen, U. G.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen O, Denmark.
[Caldwell, J.] McDonald Observ, Ft Davis, TX 79734 USA.
[Kubas, D.; Brillant, S.; Snodgrass, C.] European So Observ, Santiago 19, Chile.
[Han, C.] Chungbuk Natl Univ, Dept Phys, Inst Basic Sci Res, Chonju 361763, South Korea.
[Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Abe, F.; Fukui, A.; Furusawa, K.; Hosaka, S.; Itow, Y.; Kamiya, K.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Nagaya, M.; Nishimoto, K.; Okumura, T.; Sumi, T.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Botzler, C. S.; Douchin, D.; Freeman, M.; Perrott, Y. C.; Rattenbury, N.; Von Seggern, E.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland, New Zealand.
[Kilmartin, P. M.; Tristram, P. J.] Mt John Observ, Lake Tekapo 8780, New Zealand.
[Korpela, A.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan.
[Calitz, J. J.; Hoffman, M.; Meintjes, P.] Univ Free State, Fac Nat & Agr Sci, Dept Phys, ZA-9300 Bloemfontein, South Africa.
[Cole, A.; Greenhill, J.; Watson, R.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Cook, K.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA.
[Coutures, C.] CEA Saclay, F-91191 Gif Sur Yvette, France.
[Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia.
[Donatowicz, J.] Vienna Univ Technol, A-1040 Vienna, Austria.
Univ Toulouse, CNRS, LATT, Toulouse, France.
[Jablonski, F.; Martioli, E.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, SP, Brazil.
[Kane, S. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia.
[Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Wambsganss, J.; Zub, M.; Liebig, C.; Maier, G.; Zimmer, F.] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany.
[Zub, M.] Univ Zielona Gora, Inst Astron, PL-65265 Zielona Gora, Poland.
[Allen, W.] Vintage Lane Observ, Blenheim, New Zealand.
[Bos, M.] Molehill Astron Observ, Auckland, New Zealand.
[Depoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX USA.
[Drummond, J.] Possum Observ, Patutahi, New Zealand.
[Gal-Yam, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Higgins, D.] Hunters Hill Observ, Canberra, ACT, Australia.
[Gorbikov, E.; Kaspi, S.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Lee, C. -U.; Park, B. -G.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Mallia, F.; Maury, A.] Campo Catino Austral Observ, San Pedro De Atacama, Chile.
[Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand.
[Natusch, T.] AUT Univ, Auckland, New Zealand.
[Ofek, E. O.] Palomar Observ, San Diego, CA USA.
[Santallo, R.] So Stars Observ, Faaa, Tahiti, Fr Polynesia.
[Allan, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England.
[Kains, N.; Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[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.
Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Tsapras, Y.] Univ London, Astron Unit, Sch Math Sci, London E1 4NS, England.
[Tsapras, Y.; Street, R. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Street, R. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Novati, S. Calchi; Bozza, V.; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84085 Fisciano, SA, Italy.
[Novati, S. Calchi; Bozza, V.; Mancini, L.; Scarpetta, G.] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
[Novati, S. Calchi; Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, Catania, Italy.
[Dominik, M.] Royal Soc Univ, London, England.
[Dreizler, S.; Hessman, F. V.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran 111559161, Iran.
[Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Rahvar, S.] IPM Inst Studies Theoret Phys & Math, Sch Astron, Tehran, Iran.
[Mancini, L.] Univ Sannio, Dipartimento Ingn, I-82100 Benevento, Italy.
[An, J.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Williams, A.] Univ Western Australia, Sch Phys, Perth, WA 6009, Australia.
RP Batista, V (reprint author), Probing Lensing Anomalies NETwork PLANET, Chicago, IL USA.
EM batista@iap.fr; gould@astronomy.ohio-state.edu; dong@ias.edu;
i.a.bond@massey.ac.nz; beaulieu@iap.fr; lagmonar@nmisa.org;
gwchristie@christie.org.nz; farmcoveobs@xtra.co.nz;
Michael.Albrow@canterbury.ac.nz; caldwell@astro.as.utexas.edu;
simkoz@astronomy.ohio-state.edu; dkubas@eso.org;
gaudi@astronomy.ohio-state.edu; cheongho@astroph.chungbuk.ac.kr;
bennett@nd.edu; jinan@nao.cas.cn; abe@stelab.nagoya-u.ac.jp;
c.botzler@auckland.ac.nz; afukui@stelab.nagoya-u.ac.jp;
furusawa@stelab.nagoya-u.ac.jp; itow@stelab.nagoya-u.ac.jp;
kkamiya@stelab.nagoya-u.ac.jp; a.korpela@niwa.co.nz; w.lin@massey.ac.nz;
c.h.ling@massey.ac.nz; kmasuda@stelab.nagoya-u.ac.jp;
ymatsu@stelab.nagoya-u.ac.jp; nmiyake@stelab.nagoya-u.ac.jp;
mnagaya@stelab.nagoya-u.ac.jp; okumurat@stelab.nagoya-u.ac.jp;
yper006@auckland.ac.nz; denis.sullivan@vuw.ac.nz;
sumi@stelab.nagoya-u.ac.jp; w.sweatman@massey.ac.nz;
p.yock@auckland.ac.nz; sbrillan@eso.org; cassan@iap.fr;
Andrew.Cole@utas.edu.au; kcook@llnl.gov; coutures@iap.fr;
donatowicz@tuwien.ac.at; John.Greenhill@utas.edu.au;
HoffmaMJ.SCI@mail.uovs.ac.za; skane@ipac.caltech.edu;
nk87@st-andrews.ac.uk; marquett@iap.fr; Ralph.Martin@dec.wa.gov.au;
ep41@st-andrews.ac.uk; Andrew.Williams@dec.wa.gov.au;
whallen@xtra.co.nz; gbolt@iinet.net.au; molehill@ihug.co.nz;
depoy@physics.tamu.edu; john_drummond@xtra.co.nz;
jdeast@astronomy.ohio-state.edu; avishay.gal-yam@weizmann.ac.il;
dhi67540@bigpond.net.au; leecu@kasi.re.kr;
francomallia@campocatinobservatory.org; alain@spaceobs.com;
lagmonar@nmisa.org; acrux@orcon.net.nz; nick.morgan@alum.mit.edu;
tim.natusch@aut.ac.nz; eran@astro.caltech.edu; bgpark@kasi.re.kr;
pogge@astronomy.ohio-state.edu; obs930@southernstars-observatory.org;
shporer@wise.tau; odedspec@wise.tau; guy.thornley@gmail.com;
jyee@astronomy.ohio-state.edu
RI Zimmer, Fabian/M-4765-2014; Hundertmark, Markus/C-6190-2015; Rahvar,
Sohrab/A-9350-2008; Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012;
Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013; Kozlowski,
Szymon/G-4799-2013; 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013;
Williams, Andrew/K-2931-2013
OI Cole, Andrew/0000-0003-0303-3855; Ricci, Davide/0000-0002-9790-0552;
Snodgrass, Colin/0000-0001-9328-2905; Hundertmark,
Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Eastman,
Jason/0000-0003-3773-5142; Dominik, Martin/0000-0002-3202-0343;
Kozlowski, Szymon/0000-0003-4084-880X; Williams,
Andrew/0000-0001-9080-0105
FU HOLMES [ANR-06-BLAN-0416]; NSF [AST-0757888, AST-0206189, AST-0708890];
NASA [NNG04GL51G, NAF5-13042, NNX07AL71G]; Polish MNiSW [N20303032/4275,
HST-GO-11311]; Korea Science and Engineering Foundation [2009-008561];
Korea Research Foundation [2006-311-C00072]; Korea Astronomy and Space
Science Institute (KASI); Deutsche Forschungsgemeinschaft; PPARC/STFC;
EU; Dill Faulkes Educational Trust (Faulkes Telescope North); Marsden
Fund of NZ; Foundation for Research Science and Technology of NZ;
Creative Research Initiative program [2009-008561]; Chinese Academy of
Sciences (CAS) [2009Y2AJ7]; [JSPS18253002]; [JSPS20340052];
[JSPS19340058]; [MEXT19015005]; [JSPS18749004]
FX V.B. thanks Ohio State University for its hospitality during a six week
visit, during which this study was initiated. We acknowledge the
following support: Grants HOLMES ANR-06-BLAN-0416 Dave Warren for the Mt
Canopus Observatory; NSF AST-0757888 (AG, SD); NASA NNG04GL51G (DD, AG,
RP); Polish MNiSW N20303032/4275 (AU); HST-GO-11311 (KS); NSF
AST-0206189 and AST-0708890, NASA NAF5-13042 and NNX07AL71G (DPB); Korea
Science and Engineering Foundation grant 2009-008561 (CH); Korea
Research Foundation grant 2006-311-C00072 (B-GP); Korea Astronomy and
Space Science Institute (KASI); Deutsche Forschungsgemeinschaft (CSB);
PPARC/STFC, EU FP6 programme "ANGLES" (LW, NJR); PPARC/STFC (RoboNet);
Dill Faulkes Educational Trust (Faulkes Telescope North); Grants
JSPS18253002, JSPS20340052 and JSPS19340058 (MOA); Marsden Fund of
NZ(IAB, PCMY); Foundation for Research Science and Technology of NZ;
Creative Research Initiative program (2009-008561) (CH); Grants
MEXT19015005 and JSPS18749004 (TS). Work by S. D. was performed under
contract with the California Institute of Technology (Caltech) funded by
NASA through the Sagan Fellowship Program. J.C.Y. is supported by an NSF
Graduate Research Fellowship. This work was supported in part by an
allocation of computing time from the Ohio Supercomputer Center. J.A. is
supported by the Chinese Academy of Sciences (CAS) Fellowships for Young
International Scientist, Grant No.: 2009Y2AJ7.
NR 48
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2011
VL 529
AR A102
DI 10.1051/0004-6361/201016111
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 750OG
UT WOS:000289557200110
ER
PT J
AU Berger, JP
Monnier, JD
Millan-Gabet, R
Renard, S
Pedretti, E
Traub, W
Bechet, C
Benisty, M
Carleton, N
Haguenauer, P
Kern, P
Labeye, P
Longa, F
Lacasse, M
Malbet, F
Perraut, K
Ragland, S
Schloerb, P
Schuller, PA
Thiebaut, E
AF Berger, J. -P.
Monnier, J. D.
Millan-Gabet, R.
Renard, S.
Pedretti, E.
Traub, W.
Bechet, C.
Benisty, M.
Carleton, N.
Haguenauer, P.
Kern, P.
Labeye, P.
Longa, F.
Lacasse, M.
Malbet, F.
Perraut, K.
Ragland, S.
Schloerb, P.
Schuller, P. A.
Thiebaut, E.
TI First astronomical unit scale image of the GW Orionis triple system
Direct detection of a new stellar companion
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE binaries: general; stars: variables: T Tauri; Herbig Ae/Be; accretion,
accretion disks; techniques: interferometric
ID INTERFEROMETRY; ACCRETION; EVOLUTION; DISTANCE; NEBULA; TRACKS; STARS;
IOTA
AB Context. Young and close multiple systems are unique laboratories to probe the initial dynamical interactions between forming stellar systems and their dust and gas environment. Their study is a key building block to understanding the high frequency of main-sequence multiple systems. However, the number of detected spectroscopic young multiple systems that allow dynamical studies is limited. GW Orionis is one such system. It is one of the brightest young T Tauri stars and is surrounded by a massive disk.
Aims. Our goal is to probe the GW Orionis multiplicity at angular scales at which we can spatially resolve the orbit.
Methods. We used the IOTA/IONIC3 interferometer to probe the environment of GW Orionis with an astronomical unit resolution in 2003, 2004, and 2005. By measuring squared visibilities and closure phases with a good UV coverage we carry out the first image reconstruction of GW Ori from infrared long-baseline interferometry.
Results. We obtained the first infrared image of a T Tauri multiple system with astronomical unit resolution. We show that GW Orionis is a triple system, resolve for the first time the previously known inner pair (separation rho similar to 1.4 AU) and reveal a new more distant component (GW Ori C) with a projected separation of similar to 8 AU with direct evidence of motion. Furthermore, the nearly equal (2: 1) H-band flux ratio of the inner components suggests that either GW Ori B is undergoing a preferential accretion event that increases its disk luminosity or that the estimate of the masses has to be revisited in favour of a more equal mass-ratio system that is seen at lower inclination.
Conclusions. Accretion disk models of GW Ori will need to be completely reconsidered because of this outer companion C and the unexpected brightness of companion B.
C1 [Berger, J. -P.; Haguenauer, P.] European So Observ, Santiago 19, Chile.
[Berger, J. -P.; Renard, S.; Kern, P.; Longa, F.; Malbet, F.; Perraut, K.] Univ Grenoble 1, IPAG, CNRS UMR 5571, F-38041 Grenoble, France.
[Monnier, J. D.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Millan-Gabet, R.] CALTECH, Pasadena, CA 91125 USA.
[Pedretti, E.] Univ St Andrews, St Andrews KY16 9AJ, Fife, Scotland.
[Traub, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Benisty, M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Carleton, N.; Lacasse, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Labeye, P.] CEA DRT LETI, F-38054 Grenoble, France.
[Ragland, S.] WM Keck Observ, Kamuela, HI 96743 USA.
[Schloerb, P.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Schuller, P. A.] Univ Paris 11, CNRS UMR 8617, IAS, F-91405 Orsay, France.
[Bechet, C.; Thiebaut, E.] CRAL Observ Lyon, F-69561 St Genis Laval, France.
RP Berger, JP (reprint author), European So Observ, Alonso de Cordova 3107 Vitacura,Casilla 19001, Santiago 19, Chile.
EM jpberger@eso.org
RI Bechet, Clementine/A-6828-2017
OI Bechet, Clementine/0000-0002-0885-3644
FU ASHRA; PNPS/INSU; Michelson fellowship program; CNRS; CNES
FX This work was supported by ASHRA, PNPS/INSU, and Michelson fellowship
program. This research has made use of the SIMBAD database, operated at
CDS, Strasbourg, France and getCal software from the NASA Exoplanet
Science Institute, Caltech. Bibliographic references were provided by
the SAO/NASA Astrophysics Data System. IONIC-3 has been developed by
LAOG and CEA-LETI, and funded by the CNRS and CNES. We thank Russel
White, Lee Hartmann and S. Meimon for useful discussions.
NR 18
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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 MAY
PY 2011
VL 529
AR L1
DI 10.1051/0004-6361/201016219
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 750OG
UT WOS:000289557200002
ER
PT J
AU Bouwman, J
Cuppen, HM
Steglich, M
Allamandola, LJ
Linnartz, H
AF Bouwman, J.
Cuppen, H. M.
Steglich, M.
Allamandola, L. J.
Linnartz, H.
TI Photochemistry of polycyclic aromatic hydrocarbons in cosmic water ice
II. Near UV/VIS spectroscopy and ionization rates
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrochemistry; molecular processes; methods: laboratory; techniques:
spectroscopic; ISM: molecules
ID YOUNG STELLAR OBJECTS; H2O INTERSTELLAR ICE; RADICAL CATIONS; OPTICAL
SPECTROSCOPY; VIBRATIONAL-SPECTRA; ASTROPHYSICAL ICES;
EXCITATION-SPECTRA; FACILE GENERATION; CORONENE CATION; EXCITED-STATES
AB Context. Mid-infrared emission features originating from polycyclic aromatic hydrocarbons (PAHs) are observed towards photon dominated regions in space. Towards dense clouds, however, these emission features are quenched. Observations of dense clouds show that many simple volatile molecules are frozen out on interstellar grains, forming thin layers of ice. Recently, observations have shown that more complex non-volatile species, presumably including PAHs, also freeze out and contribute to the ongoing solid-state chemistry.
Aims. The study presented here aims at obtaining reaction rate data that characterize PAH photochemistry upon vacuum ultraviolet (VUV) irradiation in an interstellar H(2)O ice analogue to explore the potential impact of PAH:H(2)O ice reactions on overall interstellar ice chemistry. To this end, the experimental results are implemented in a chemical model under simple interstellar cloud conditions.
Methods. Time-dependent near-UV/VIS spectroscopy on the VUV photochemistry of anthracene, pyrene, benzo[ghi]perylene and coronene containing interstellar H(2)O ice analogs is performed at 25 and 125 K, using an optical absorption setup.
Results. Near-UV/VIS absorption spectra are presented for these four PAHs and their photoproducts including cationic species trapped in H(2)O ice. Oscillator strengths of the cation absorption bands are derived relative to the oscillator strength of the neutral parent PAH. The loss of the parent and growth of PAH photoproducts are measured as a function of VUV dose, yielding solid state reaction constants. The rate constants are used in an exploratory astrochemical model, to assess the importance of PAH:H(2)O ice photoprocessing in UV exposed interstellar environments, compared with the timescales in which PAH molecules are incorporated in interstellar ices.
Conclusions. All four PAHs studied here are found to be readily ionized upon VUV photolysis when trapped in H(2)O ice and exhibit similar rates for ionization at astronomically relevant temperatures. Depending on the relative efficiency of H(2)O photodesorption and PAH photoionization in H(2)O ice, the latter may trigger a charge induced aromatic solid state chemistry, in which PAH cations play a central role.
C1 [Steglich, M.] Univ Jena, Lab Astrophys Grp, Max Planck Inst Astron, Inst Solid State Phys, D-07743 Jena, Germany.
[Allamandola, L. J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Bouwman, J.; Cuppen, H. M.; Linnartz, H.] Leiden Univ, Leiden Observ, Raymond & Beverly Sackler Lab Astrophys, NL-2300 RA Leiden, Netherlands.
RP Bouwman, J (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
EM bouwman@berkeley.edu
RI Cuppen, Herma/F-9729-2015;
OI Cuppen, Herma/0000-0003-4397-0739; Steglich, Mathias/0000-0001-8206-6588
FU "Stichting voor Fundamenteel Onderzoek der Materie" (FOM); "the
Netherlands Research School for Astronomy" (NOVA); NASA's Laboratory;
European Community [238258]
FX This work is financially supported by "Stichting voor Fundamenteel
Onderzoek der Materie" (FOM), "the Netherlands Research School for
Astronomy" (NOVA), and NASA's Laboratory Astrophysics and Astrobiology
Programs. The research leading to these results has received funding
from the [European Community's] Seventh Framework Programme
[FP7/2007-2013] under grant agreement no [238258]. The
authors would like to thank Ankan Das for his contribution to the data
reduction.
NR 46
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2011
VL 529
AR A46
DI 10.1051/0004-6361/201015762
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 750OG
UT WOS:000289557200054
ER
PT J
AU Faure, C
Anguita, T
Alloin, D
Bundy, K
Finoguenov, A
Leauthaud, A
Knobel, C
Kneib, JP
Jullo, E
Ilbert, O
Koekemoer, AM
Capak, P
Scoville, N
Tasca, LAM
AF Faure, C.
Anguita, T.
Alloin, D.
Bundy, K.
Finoguenov, A.
Leauthaud, A.
Knobel, C.
Kneib, J-P
Jullo, E.
Ilbert, O.
Koekemoer, A. M.
Capak, P.
Scoville, N.
Tasca, L. A. M.
TI On the evolution of environmental and mass properties of strong lens
galaxies in COSMOS
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: strong
ID DARK-MATTER HALOS; HIGH-DENSITY ENVIRONMENTS; WIDE-FIELD SURVEY; ACS
SURVEY; GRAVITATIONAL LENSES; STELLAR MASS; QUANTITATIVE MORPHOLOGY;
PHOTOMETRIC REDSHIFTS; INTERNAL STRUCTURE; OPTICAL DEPTHS
AB Context. Nearly 100 new strong-lens candidates have been discovered in the COSMOS field. Among these, 20 lens candidates with 0.34 less than or similar to z(lens) <= 1.13 feature multiple images of background sources.
Aims. Using the multi-wavelength coverage of the field and its spectroscopic follow-up, we characterize the evolution with redshift of the environment and of the dark-matter (DM) fraction of the lens galaxies.
Methods. We present spectroscopic and new photometric redshifts of the strong-lens candidates. The lens environment is characterized in the following way: we account for the projected 10 closest galaxies around each lens and for galaxies with a projected distance less than 1 Mpc at the lens galaxy redshift. In both cases, we perform similar measurements on a control sample of "twin" non-lens early-type galaxies (ETGs). In addition, we identify group members and field galaxies in the X-ray and optical catalogs of galaxy groups and clusters. From those catalogs, we measure the external shear contribution of the groups/clusters surrounding the lens galaxies. The systems are then modeled using a singular isothermal ellipsoid for the lens galaxies plus the external shear produced by the groups/clusters.
Results. We observe that the average stellar mass of lens galaxies increases with redshift. In addition, we measure that the environment of lens galaxies is compatible with that of the twins over the whole redshift range tested here. During the lens modeling, we notice that when let free, the external shear points in a direction which is the mean direction of the external shear produced by the groups/clusters and of the closest galaxy to the lens. We also notice that the DM fraction of the lens galaxies measured within the Einstein radius significantly decreases as the redshift increases.
Conclusions. Given these observations, we conclude that while the environment of lens galaxies is compatible with that of non-lens ETGS over a wide range of redshifts, their mass properties evolves significantly with redshift: it is still not clear whether this advocates in favor of a stronger lensing bias toward massive objects at high redshift or if it is simply representative of the high proportion of massive and high stellar density galaxies at high redshift.
C1 [Faure, C.] Observ Sauverny, Ecole Polytech Fed Lausanne, Astrophys Lab, CH-1290 Versoix, Switzerland.
[Anguita, T.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Ctr Astroingn, Santiago, Chile.
[Anguita, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Alloin, D.] Univ Paris Diderot, CNRS, Lab AIM, CEA,DSM,IRFU,SEDI,SAP,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Bundy, K.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Finoguenov, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Leauthaud, A.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Leauthaud, A.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Knobel, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Kneib, J-P; Ilbert, O.; Tasca, L. A. M.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Jullo, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Capak, P.; Scoville, N.] CALTECH, Pasadena, CA 91125 USA.
RP Faure, C (reprint author), Observ Sauverny, Ecole Polytech Fed Lausanne, Astrophys Lab, CH-1290 Versoix, Switzerland.
RI Kneib, Jean-Paul/A-7919-2015;
OI Kneib, Jean-Paul/0000-0002-4616-4989; Koekemoer,
Anton/0000-0002-6610-2048
FU CNRS; CEA; SL2S [ANR-06-BLAN-0067]; DESIR [ANR-07-BLAN-0228]; NPP; NASA
FX We acknowledge the anonymous referee for providing a detailed and very
useful report. We are gratefully indebted to M. Limousin and R. Gavazzi
for enlightening discussions. D.A. thanks CNRS and CEA for support and
visits to the Geneva observatory, where this work was finalized. J.P.K.
thanks for support from CNRS and SL2S ANR-06-BLAN-0067 and DESIR
ANR-07-BLAN-0228. E.J. acknowledges the support of the NPP, administered
by Oak Ridge Associated Universities through a contract with NASA.
NR 68
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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 MAY
PY 2011
VL 529
AR A72
DI 10.1051/0004-6361/200913498
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 750OG
UT WOS:000289557200080
ER
PT J
AU Guilbert-Lepoutre, A
Lasue, J
Federico, C
Coradini, A
Orosei, R
Rosenberg, ED
AF Guilbert-Lepoutre, A.
Lasue, J.
Federico, C.
Coradini, A.
Orosei, R.
Rosenberg, E. D.
TI New 3D thermal evolution model for icy bodies application to
trans-Neptunian objects
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Kuiper belt: general; diffusion; methods: numerical
ID KUIPER-BELT OBJECTS; COMET NUCLEI; SOLAR-SYSTEM; PHASE-TRANSITION;
WATER-ICE; CENTAURS; SURFACE; ORIGIN; HEAT; IRRADIATION
AB Context. Thermal evolution models have been developed over the years to investigate the evolution of thermal properties based on the transfer of heat fluxes or transport of gas through a porous matrix, among others. Applications of such models to trans-Neptunian objects (TNOs) and Centaurs has shown that these bodies could be strongly differentiated from the point of view of chemistry (i.e. loss of most volatile ices), as well as from physics (e.g. melting of water ice), resulting in stratified internal structures with differentiated cores and potential pristine material close to the surface. In this context, some observational results, such as the detection of crystalline water ice or volatiles, remain puzzling.
Aims. In this paper, we would like to present a new fully three-dimensional thermal evolution model. With this model, we aim to improve determination of the temperature distribution inside icy bodies such as TNOs by accounting for lateral heat fluxes, which have been proven to be important for accurate simulations. We also would like to be able to account for heterogeneous boundary conditions at the surface through various albedo properties, for example, that might induce different local temperature distributions.
Methods. In a departure from published modeling approaches, the heat diffusion problem and its boundary conditions are represented in terms of real spherical harmonics, increasing the numerical efficiency by roughly an order of magnitude. We then compare this new model and another 3D model recently published to illustrate the advantages and limits of the new model. We try to put some constraints on the presence of crystalline water ice at the surface of TNOs.
Results. The results obtained with this new model are in excellent agreement with results obtained by different groups with various models. Small TNOs could remain primitive unless they are formed quickly (less than 2 Myr) or are debris from the disruption of larger bodies. We find that, for large objects with a thermal evolution dominated by the decay of long-lived isotopes (objects with a formation period greater than 2 to 3 Myr), the presence of crystalline water ice would require both a large radius (>300 km) and high density (>1500 kg m(-3)). In particular, objects with intermediate radii and densities would be an interesting transitory population deserving a detailed study of individual fates.
C1 [Guilbert-Lepoutre, A.] Observ Paris, Sect Meudon, LESIA, F-92195 Meudon, France.
[Guilbert-Lepoutre, A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Lasue, J.] Los Alamos Natl Lab, ISR 1, Los Alamos, NM 87545 USA.
[Lasue, J.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Federico, C.] Univ Perugia, Dipartimento Sci Terra, I-06123 Perugia, Italy.
[Coradini, A.] INAF IFSI, I-00133 Rome, Italy.
[Orosei, R.] INAF IASF, I-00133 Rome, Italy.
[Rosenberg, E. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Guilbert-Lepoutre, A (reprint author), Observ Paris, Sect Meudon, LESIA, 2 Pl J Janssen, F-92195 Meudon, France.
EM aguilbert@ucla.edu
FU NASA
FX A.G.L. thanks G. Magni, M. T. Capria, M. C. De Sanctis and D. Turini for
useful discussions on the model, and D. Jewitt for useful comments on
the manuscript. J.L. thanks the LPI contribution 1549. A.G.L. was
supported in part by a NASA Herschel grant to David Jewitt. The authors
want to thank the anonymous referee for their useful comments that
contributed to a major improvement of the manuscript.
NR 64
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FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2011
VL 529
AR A71
DI 10.1051/0004-6361/201014194
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 750OG
UT WOS:000289557200079
ER
PT J
AU Marshall, JP
Lohne, T
Montesinos, B
Krivov, AV
Eiroa, C
Absil, O
Bryden, G
Maldonado, J
Mora, A
Sanz-Forcada, J
Ardila, D
Augereau, JC
Bayo, A
del Burgo, C
Danchi, W
Ertel, S
Fedele, D
Fridlund, M
Lebreton, J
Gonzalez-Garcia, BM
Liseau, R
Meeus, G
Muller, S
Pilbratt, GL
Roberge, A
Stapelfeldt, K
Thebault, P
White, GJ
Wolf, S
AF Marshall, J. P.
Loehne, T.
Montesinos, B.
Krivov, A. V.
Eiroa, C.
Absil, O.
Bryden, G.
Maldonado, J.
Mora, A.
Sanz-Forcada, J.
Ardila, D.
Augereau, J. -Ch.
Bayo, A.
del Burgo, C.
Danchi, W.
Ertel, S.
Fedele, D.
Fridlund, M.
Lebreton, J.
Gonzalez-Garcia, B. M.
Liseau, R.
Meeus, G.
Mueller, S.
Pilbratt, G. L.
Roberge, A.
Stapelfeldt, K.
Thebault, P.
White, G. J.
Wolf, S.
TI A Herschel resolved far-infrared dust ring around HD 207129
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: individual: HD 207129; circumstellar matter; infrared: stars
ID MAIN-SEQUENCE STARS; VEGA-TYPE STARS; NEARBY STARS; DEBRIS DISKS;
BETA-PICTORIS; Q(1) ERIDANI; PLANET; SEARCH; SPACE; BELT
AB Context. Dusty debris discs around main sequence stars are thought to be the result of continuous collisional grinding of planetesimals in the system. The majority of these systems are unresolved and analysis of the dust properties is limited by the lack of information regarding the dust location.
Aims. The Herschel DUNES key program is observing 133 nearby, Sun-like stars (<20 pc, FGK spectral type) in a volume limited survey to constrain the absolute incidence of cold dust around these stars by detection of far infrared excess emission at flux levels comparable to the Edgeworth-Kuiper belt (EKB).
Methods. We have observed the Sun-like star HD 207129 with Herschel PACS and SPIRE. In all three PACS bands we resolve a ring-like structure consistent with scattered light observations. Using alpha Bootis as a reference point spread function (PSF), we deconvolved the images, clearly resolving the inner gap in the disc at both 70 and 100 mu m.
Results. We have resolved the dust-producing planetesimal belt of a debris disc at 100 mu m for the first time. We measure the radial profile and fractional luminosity of the disc, and compare the values to those of discs around stars of similar age and/or spectral type, placing this disc in context of other resolved discs observed by Herschel/DUNES.
C1 [Marshall, J. P.; Eiroa, C.; Maldonado, J.; Mora, A.; Fedele, D.; Meeus, G.] Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain.
[Loehne, T.; Krivov, A. V.; Mueller, S.] Univ Jena, Inst Astrophys, D-07743 Jena, Germany.
[Loehne, T.; Krivov, A. V.; Mueller, S.] Univ Sternwarte, D-07743 Jena, Germany.
[Montesinos, B.; Sanz-Forcada, J.] CSIC INTA, CAB, Ctr Astrobiol, Dept Astrofis, Madrid 28691, Spain.
[Absil, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium.
[Bryden, G.; Stapelfeldt, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain.
[Ardila, D.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Augereau, J. -Ch.; Lebreton, J.] UJF Grenoble 1 CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France.
[Bayo, A.] European Space Observ, Santiago 19, Chile.
[del Burgo, C.] UNINOVA CA3, P-2825149 Caparica, Portugal.
[Danchi, W.; Roberge, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ertel, S.; Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany.
[Fedele, D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Fedele, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21210 USA.
[Fridlund, M.; Pilbratt, G. L.] ESTEC SRE SA, ESA Astrophys & Fundamental Phys Missions Div, NL-2201 AZ Noordwijk, Netherlands.
[Gonzalez-Garcia, B. M.] ESAC, INSA, Madrid 28691, Spain.
[Liseau, R.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden.
[Thebault, P.] Observ Paris, LESIA, F-92195 Meudon, France.
[White, G. J.] Open Univ, Dept Phys & Astrophys, Milton Keynes MK7 6AA, Bucks, England.
[White, G. J.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
RP Marshall, JP (reprint author), Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain.
EM jonathan.marshall@uam.es
RI Roberge, Aki/D-2782-2012; Stapelfeldt, Karl/D-2721-2012; Fedele,
Davide/L-8688-2013; Sanz-Forcada, Jorge/C-3176-2017; Montesinos,
Benjamin/C-3493-2017;
OI Roberge, Aki/0000-0002-2989-3725; Fedele, Davide/0000-0001-6156-0034;
Sanz-Forcada, Jorge/0000-0002-1600-7835; Montesinos,
Benjamin/0000-0002-7982-2095; Marshall, Jonathan/0000-0001-6208-1801
FU Spanish grant [AYA 2008/01727]; DFG [Lo 1715/1-1, Kr 2164/9-1]; CNES-PNP
FX We would like to thank the staff at the Herschel Science Centre,
discussions with whom added immeasurably to the quality of the data
reduction. C. Eiroa, J. Maldonado, J. P. Marshall, and B. Montesinos are
partly supported by Spanish grant AYA 2008/01727. T. Lohne, S. Muller
and A. Krivov acknowledge support by the DFG, projects Lo 1715/1-1 and
Kr 2164/9-1. J.-Ch. Augereau, J. Lebreton and P. Thebault are supported
by a CNES-PNP grant.
NR 46
TC 28
Z9 28
U1 0
U2 8
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2011
VL 529
AR A117
DI 10.1051/0004-6361/201116673
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 750OG
UT WOS:000289557200125
ER
PT J
AU Abbasi, R
Abdou, Y
Abu-Zayyad, T
Adams, J
Aguilar, JA
Ahlers, M
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Bay, R
Alba, JLB
Beattie, K
Beatty, JJ
Bechet, S
Becker, JK
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Braun, J
Brown, AM
Buitink, S
Carson, M
Chirkin, D
Christy, B
Clem, J
Clevermann, F
Cohen, S
Colnard, C
Cowen, DF
D'Agostino, MV
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
Demirors, L
Depaepe, O
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dierckxsens, M
Dreyer, J
Dumm, JP
Ehrlich, R
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feusels, T
Filimonov, K
Finley, C
Foerster, MM
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Geisler, M
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Grant, D
Griesel, T
Gross, A
Grullon, S
Gurtner, M
Ha, C
Hallgren, A
Halzen, F
Han, K
Hanson, K
Helbing, K
Herquet, P
Hickford, S
Hill, GC
Hoffman, KD
Homeier, A
Hoshina, K
Hubert, D
Huelsnitz, W
Hulss, JP
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kemming, N
Kenny, P
Kiryluk, J
Kislat, F
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Koskinen, DJ
Kowalski, M
Kowarik, T
Krasberg, M
Krings, T
Kroll, G
Kuehn, K
Kuwabara, T
Labare, M
Lafebre, S
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lehmann, R
Lunemann, J
Madsen, J
Majumdar, P
Marotta, A
Maruyama, R
Mase, K
Matis, HS
Matusik, M
Meagher, K
Merck, M
Meszaros, P
Meures, T
Middell, E
Milke, N
Miller, J
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Nam, JW
Naumann, U
Niessen, P
Nygren, DR
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Ono, M
Panknin, S
Paul, L
de los Heros, CP
Petrovic, J
Piegsa, A
Pieloth, D
Porrata, R
Posselt, J
Price, PB
Prikockis, M
Przybylski, GT
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Rodrigues, JP
Roth, P
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Schlenstedt, S
Schmidt, T
Schukraft, A
Schultes, A
Schulz, O
Schunck, M
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Singh, K
Slipak, A
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stephens, G
Stezelberger, T
Stokstad, RG
Stoyanov, S
Strahler, EA
Straszheim, T
Sullivan, GW
Swillens, Q
Taavola, H
Taboada, I
Tamburro, A
Tarasova, O
Tepe, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Tosi, D
Turcan, D
van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Voigt, B
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wischnewski, R
Wissing, H
Wolf, M
Woschnagg, K
Xu, C
Xu, XW
Yodh, G
Yoshida, S
Zarzhitsky, P
AF Abbasi, R.
Abdou, Y.
Abu-Zayyad, T.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Bay, R.
Alba, J. L. Bazo
Beattie, K.
Beatty, J. J.
Bechet, S.
Becker, J. K.
Becker, K-H
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brown, A. M.
Buitink, S.
Carson, M.
Chirkin, D.
Christy, B.
Clem, J.
Clevermann, F.
Cohen, S.
Colnard, C.
Cowen, D. F.
D'Agostino, M. V.
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
Demiroers, L.
Depaepe, O.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dierckxsens, M.
Dreyer, J.
Dumm, J. P.
Ehrlich, R.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feusels, T.
Filimonov, K.
Finley, C.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Geisler, M.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Grant, D.
Griesel, T.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Helbing, K.
Herquet, P.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Homeier, A.
Hoshina, K.
Hubert, D.
Huelsnitz, W.
Huelss, J-P
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Joseph, J. M.
Kampert, K-H
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
Kemming, N.
Kenny, P.
Kiryluk, J.
Kislat, F.
Klein, S. R.
Koehne, J-H
Kohnen, G.
Kolanoski, H.
Koepke, L.
Koskinen, D. J.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Krings, T.
Kroll, G.
Kuehn, K.
Kuwabara, T.
Labare, M.
Lafebre, S.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Lehmann, R.
Luenemann, J.
Madsen, J.
Majumdar, P.
Marotta, A.
Maruyama, R.
Mase, K.
Matis, H. S.
Matusik, M.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Middell, E.
Milke, N.
Miller, J.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Nam, J. W.
Naumann, U.
Niessen, P.
Nygren, D. R.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Ono, M.
Panknin, S.
Paul, L.
de los Heros, C. Perez
Petrovic, J.
Piegsa, A.
Pieloth, D.
Porrata, R.
Posselt, J.
Price, P. B.
Prikockis, M.
Przybylski, G. T.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Rodrigues, J. P.
Roth, P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Sander, H-G
Santander, M.
Sarkar, S.
Schatto, K.
Schlenstedt, S.
Schmidt, T.
Schukraft, A.
Schultes, A.
Schulz, O.
Schunck, M.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Singh, K.
Slipak, A.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stephens, G.
Stezelberger, T.
Stokstad, R. G.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Sullivan, G. W.
Swillens, Q.
Taavola, H.
Taboada, I.
Tamburro, A.
Tarasova, O.
Tepe, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Tosi, D.
Turcan, D.
van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Voigt, B.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Wolf, M.
Woschnagg, K.
Xu, C.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
CA IceCube Collaboration
TI TIME-INTEGRATED SEARCHES FOR POINT-LIKE SOURCES OF NEUTRINOS WITH THE
40-STRING IceCube DETECTOR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; cosmic rays; neutrinos
ID HIGH-ENERGY NEUTRINOS; GAMMA-RAY EMISSION; COSMIC-RAYS; GALAXIES;
CLUSTERS; TELESCOPES; ASTRONOMY; ASTROPHYSICS; SELECTION; MILAGRO
AB We present the results of time-integrated searches for astrophysical neutrino sources in both the northern and southern skies. Data were collected using the partially completed IceCube detector in the 40-string configuration recorded between 2008 April 5 and 2009 May 20, totaling 375.5 days livetime. An unbinned maximum likelihood ratio method is used to search for astrophysical signals. The data sample contains 36,900 events: 14,121 from the northern sky, mostly muons induced by atmospheric neutrinos, and 22,779 from the southern sky, mostly high-energy atmospheric muons. The analysis includes searches for individual point sources and stacked searches for sources in a common class, sometimes including a spatial extent. While this analysis is sensitive to TeV-PeV energy neutrinos in the northern sky, it is primarily sensitive to neutrinos with energy greater than about 1 PeV in the southern sky. No evidence for a signal is found in any of the searches. Limits are set for neutrino fluxes from astrophysical sources over the entire sky and compared to predictions. The sensitivity is at least a factor of two better than previous searches (depending on declination), with 90% confidence level muon neutrino flux upper limits being between E(2)d Phi/dE similar to 2-200 x 10(-12) TeV cm(-2) s(-1) in the northern sky and between 3-700 x 10(-12) TeV cm(-2) s(-1) in the southern sky. The stacked source searches provide the best limits to specific source classes. The full IceCube detector is expected to improve the sensitivity to d Phi/dE proportional to E-2 sources by another factor of two in the first year of operation.
C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Braun, J.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kelley, J. L.; Krasberg, M.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium.
[Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Adams, J.; Brown, A. M.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch, New Zealand.
[Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Auffenberg, J.; Becker, K-H; Gurtner, M.; Helbing, K.; Kampert, K-H; Karg, T.; Matusik, M.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schlenstedt, S.; Spiering, C.; Tarasova, O.; Tosi, D.; Voigt, B.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
[Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium.
[Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Huelss, J-P; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Deptartment Phys, SE-10691 Stockholm, Sweden.
[Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Singh, K.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Clevermann, F.; Koehne, J-H; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H-G; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Kappes, A.; Kemming, N.; Kolanoski, H.; Lehmann, R.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
RI Taavola, Henric/B-4497-2011; Beatty, James/D-9310-2011; Wiebusch,
Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Tamburro,
Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren,
Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014;
Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015;
Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011
OI Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft,
Anne/0000-0002-9112-5479; Perez de los Heros,
Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810;
Buitink, Stijn/0000-0002-6177-497X; Hubert, Daan/0000-0002-4365-865X;
Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Carson,
Michael/0000-0003-0400-7819; Beatty, James/0000-0003-0481-4952; Actis,
Oxana/0000-0001-8851-3983; Wiebusch, Christopher/0000-0002-6418-3008;
Auffenberg, Jan/0000-0002-1185-9094; Koskinen,
David/0000-0002-0514-5917; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Sarkar, Subir/0000-0002-3542-858X
FU U.S. National Science Foundation; U.S. National Science
Foundation-Physics Division; University of Wisconsin Alumni Research
Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at
the University of Wisconsin-Madison; Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy; National Energy Research
Scientific Computing Center; Louisiana Optical Network Initiative (LONI)
grid computing resources; National Science and Engineering Research
Council of Canada; Swedish Research Council; Swedish Polar Research
Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut
and Alice Wallenberg Foundation, Sweden; German Ministry for Education
and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research
Department of Plasmas with Complex Interactions (Bochum), Germany; Fund
for Scientific Research (FNRS-FWO); FWO Odysseus Programme; Flanders
Institute to encourage scientific and technological research in industry
(IWT); Belgian Federal Science Policy Office (Belspo); University of
Oxford, UK; Marsden Fund, New Zealand; Japan Society for Promotion of
Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland;
EU; Capes Foundation, Ministry of Education of Brazil
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; National Science and Engineering
Research Council of Canada; Swedish Research Council, Swedish Polar
Research Secretariat, Swedish National Infrastructure for Computing
(SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for Scientific Research
(FNRS-FWO), FWO Odysseus Programme, Flanders Institute to encourage
scientific and technological research in industry (IWT), Belgian Federal
Science Policy Office (Belspo); University of Oxford, UK; Marsden Fund,
New Zealand; Japan Society for Promotion of Science (JSPS); the Swiss
National Science Foundation (SNSF), Switzerland; A. Gross acknowledges
support by the EU Marie Curie OIF Program; J. P. Rodrigues acknowledges
support by the Capes Foundation, Ministry of Education of Brazil.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2011
VL 732
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DI 10.1088/0004-637X/732/1/18
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500018
ER
PT J
AU Ballard, S
Christiansen, JL
Charbonneau, D
Deming, D
Holman, MJ
A'Hearn, MF
Wellnitz, DD
Barry, RK
Kuchner, MJ
Livengood, TA
Hewagama, T
Sunshine, JM
Hampton, DL
Lisse, CM
Seager, S
Veverka, JF
AF Ballard, Sarah
Christiansen, Jessie L.
Charbonneau, David
Deming, Drake
Holman, Matthew J.
A'Hearn, Michael F.
Wellnitz, Dennis D.
Barry, Richard K.
Kuchner, Marc J.
Livengood, Timothy A.
Hewagama, Tilak
Sunshine, Jessica M.
Hampton, Don L.
Lisse, Carey M.
Seager, Sara
Veverka, Joseph F.
TI A SEARCH FOR ADDITIONAL PLANETS IN FIVE OF THE EXOPLANETARY SYSTEMS
STUDIED BY THE NASA EPOXI MISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; techniques: image processing; techniques:
photometric
ID TRANSIT LIGHT-CURVE; DEEP IMPACT MISSION; GIANT PLANET; KEPLER FIELD;
HOT JUPITER; TRES-2; PARAMETERS; STAR; DYNAMICS; HAT-P-7B
AB We present time series photometry and constraints on additional planets in five of the exoplanetary systems studied by the EPOCh (Extrasolar Planet Observation and Characterization) component of the NASA EPOXI mission: HAT-P-4, TrES-3, TrES-2, WASP-3, and HAT-P-7. We conduct a search of the high-precision time series for photometric transits of additional planets. We find no candidate transits with significance higher than our detection limit. From Monte Carlo tests of the time series using putative periods from 0.5 days to 7 days, we demonstrate the sensitivity to detect Neptune-sized companions around TrES-2, sub-Saturn-sized companions in the HAT-P-4, TrES-3, and WASP-3 systems, and Saturn-sized companions around HAT-P-7. We investigate in particular our sensitivity to additional transits in the dynamically favorable 3: 2 and 2: 1 exterior resonances with the known exoplanets: if we assume coplanar orbits with the known planets, then companions in these resonances with HAT-P-4b, WASP-3b, and HAT-P-7b would be expected to transit, and we can set lower limits on the radii of companions in these systems. In the nearly grazing exoplanetary systems TrES-3 and TrES-2, additional coplanar planets in these resonances are not expected to transit. However, we place lower limits on the radii of companions that would transit if the orbits were misaligned by 2 degrees.0 and 1 degrees.4 for TrES-3 and TrES-2, respectively.
C1 [Ballard, Sarah; Charbonneau, David; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Christiansen, Jessie L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Deming, Drake; Barry, Richard K.; Kuchner, Marc J.; Livengood, Timothy A.; Hewagama, Tilak] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[A'Hearn, Michael F.; Wellnitz, Dennis D.; Hewagama, Tilak; Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Hampton, Don L.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Seager, Sara] MIT, Cambridge, MA 02139 USA.
[Veverka, Joseph F.] Cornell Univ, Dept Space Sci, Ithaca, NY 14853 USA.
RP Ballard, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM sballard@cfa.harvard.edu
RI Wellnitz, Dennis/B-4080-2012; Hewagama, T/C-8488-2012; Livengood,
Timothy/C-8512-2012; Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X
FU National Aeronautics and Space Administration [NNX08AB64A, NNX08AD05A]
FX Support for this work was provided by the EPOXI Project of the National
Aeronautics and Space Administration's Discovery Program via funding to
the Goddard Space Flight Center, and to Harvard University via
Co-operative Agreement NNX08AB64A, and to the Smithsonian Astrophysical
Observatory via Co-operative Agreement NNX08AD05A.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2011
VL 732
IS 1
AR 41
DI 10.1088/0004-637X/732/1/41
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500041
ER
PT J
AU Bhat, NDR
Cordes, JM
Cox, PJ
Deneva, JS
Hankins, TH
Lazio, TJW
McLaughlin, MA
AF Bhat, N. D. R.
Cordes, J. M.
Cox, P. J.
Deneva, J. S.
Hankins, T. H.
Lazio, T. J. W.
McLaughlin, M. A.
TI AN ARECIBO SEARCH FOR PULSARS AND TRANSIENT SOURCES IN M33
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M33); pulsars: general; pulsars: individual (Crab
pulsar, B0045+33, J0628+0909); surveys
ID GIANT PULSES; X-RAY; NEUTRON-STARS; CRAB PULSAR; GAMMA-RAY; STATISTICAL
PROPERTIES; MILLISECOND PULSARS; RADIO TRANSIENTS; TELESCOPE; GALAXIES
AB We report on a systematic and sensitive search for pulsars and transient sources in the nearby spiral galaxy M33, conducted at 1.4 GHz with the Arecibo telescope's seven-beam receiver system, ALFA. Data were searched for both periodic and aperiodic sources, up to 1000 pc cm(-3) in dispersion measure and on timescales from similar to 50 mu s to several seconds. The galaxy was sampled with 12 ALFA pointings, or 84 pixels in total, each of which was searched for 2-3 hr. We describe the observations, search methodologies, and analysis strategies applicable to multibeam systems, and comment on the data quality and statistics of spurious events that arise due to radio frequency interference. While these searches have not led to any conclusive signals of periodic or transient nature that originate in the galaxy, they illustrate some of the underlying challenges and difficulties in such searches and the efficacy of simultaneous multiple beams in the analysis of search output. The implied limits are less than or similar to 5 mu Jy Mpc(2) in luminosity (at 1400 MHz) for periodic sources in M33 with duty cycles less than or similar to 5%. For short-duration transient signals (with pulse widths less than or similar to 100 mu s), the limiting peak flux density is 100 mJy, which would correspond to a 5 sigma detection of bright giant pulses (similar to 20 kJy) from Crab-like pulsars if located at the distance of M33. We discuss the implications of our null results for various source populations within the galaxy and comment on the future prospects to conduct even more sensitive searches with the upcoming next-generation instruments including the Square Kilometer Array and its pathfinders.
C1 [Bhat, N. D. R.; Cox, P. J.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Cordes, J. M.; Deneva, J. S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Hankins, T. H.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lazio, T. J. W.] SKA Program Dev Off, Manchester M13 9PL, Lancs, England.
[McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[McLaughlin, M. A.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
RP Bhat, NDR (reprint author), Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
RI Bhat, Ramesh/B-7396-2013;
OI Cox, Peter/0000-0002-6157-3430
FU NSF [AST0807151, AST-0607492]; Swinburne University; ANSTO [06/07-O-02];
AAS; Alfred P. Sloan Fellowship; WVEPSCOR
FX We thank Arun Venkataraman for his assistance in transport of the large
data volume to Swinburne University. This research was supported by NSF
grant AST0807151 to Cornell University and an internal grant from
Swinburne University. N.D.R.B. acknowledges the support received through
the ANSTO travel grant 06/07-O-02 and a research grant from AAS, and
thanks Matthew Bailes for continued support and encouragement extended
to this project. M.A.M. is supported by an Alfred P. Sloan Fellowship
and by WVEPSCOR. T.H.H. acknowledges partial support from NSF grant
AST-0607492. We thank Willem van Straten for fruitful discussions and
Sarah Burke-Spolaor for software assistance related to event analysis.
Part of this research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. We thank the referee, Scott
Ransom, for providing comments that helped to improve the clarity of
some parts of the paper. The Arecibo Observatory is operated by the
National Astronomy and Ionosphere Center under a cooperative agreement
to Cornell University.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2011
VL 732
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500014
ER
PT J
AU Brodwin, M
Stern, D
Vikhlinin, A
Stanford, SA
Gonzalez, AH
Eisenhardt, PR
Ashby, MLN
Bautz, M
Dey, A
Forman, WR
Gettings, D
Hickox, RC
Jannuzi, BT
Jones, C
Mancone, C
Miller, ED
Moustakas, LA
Ruel, J
Snyder, G
Zeimann, G
AF Brodwin, M.
Stern, D.
Vikhlinin, A.
Stanford, S. A.
Gonzalez, A. H.
Eisenhardt, P. R.
Ashby, M. L. N.
Bautz, M.
Dey, A.
Forman, W. R.
Gettings, D.
Hickox, R. C.
Jannuzi, B. T.
Jones, C.
Mancone, C.
Miller, E. D.
Moustakas, L. A.
Ruel, J.
Snyder, G.
Zeimann, G.
TI X-RAY EMISSION FROM TWO INFRARED-SELECTED GALAXY CLUSTERS AT z > 1.4 IN
THE IRAC SHALLOW CLUSTER SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (ISCS J1432.4+3250, ISCS J1438.1+3414);
galaxies: distances and redshifts; galaxies: evolution
ID DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; VELOCITY DISPERSION; COMA
CLUSTER; MASS; TEMPERATURE; LUMINOSITY; TELESCOPE; COSMOLOGY; ROBUST
AB We report the X-ray detection of two z > 1.4 infrared-selected galaxy clusters from the IRAC Shallow Cluster Survey (ISCS). We present new data from the Hubble Space Telescope and the W. M. Keck Observatory that spectroscopically confirm cluster ISCS J1432.4+3250 at z = 1.49, the most distant of 18 confirmed z > 1 clusters in the ISCS to date. We also present new spectroscopy for ISCS J1438.1+3414, previously reported at z = 1.41, and measure its dynamical mass. Clusters ISCS J1432.4+3250 and ISCS J1438.1+3414 are detected in 36 ks and 143 ks Chandra exposures at significances of 5.2 sigma and 9.7 sigma, from which we measure total masses of log (M-200,M-LX/M-circle dot) = 14.4 +/- 0.2 and 14.35(-0.11)(+0.14), respectively. The consistency of the X-ray and dynamical properties of these high-redshift clusters further demonstrates that the ISCS is robustly detecting massive clusters to at least z = 1.5.
C1 [Brodwin, M.; Vikhlinin, A.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Snyder, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stern, D.; Eisenhardt, P. R.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stanford, S. A.; Zeimann, G.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Gonzalez, A. H.; Gettings, D.; Mancone, C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Bautz, M.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Hickox, R. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
RP Brodwin, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Moustakas, Leonidas/0000-0003-3030-2360
FU Chandra X-Ray Observatory [SV4-74018, A31]; Smithsonian Astrophysical
Observatory; NASA [G09-0150A, NAS 5-26555]; JPL/Caltech; NASA through
Space Telescope Science Institute [11597, 11663]; W. M. Keck Foundation;
U.S. Department of Energy [W-7405-ENG-48]
FX This work is based, in part, on observations obtained with the Chandra
X-Ray Observatory under contract SV4-74018, A31 with the Smithsonian
Astrophysical Observatory which operates Chandra for NASA. Support for
this research was provided by NASA grant G09-0150A. 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. Support for this work was
provided by NASA through an award issued by JPL/Caltech. This work is
based, in part, on observations made with the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555. These observations are associated
with programs 11597 and 11663. Support for programs 11597 and 11663 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) and the Deep Lens Survey (DLS) 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.; This paper would not have been
possible without the efforts of the Spitzer, Chandra, HST, and Keck
support staff. We thank C. Fedeli for helpful discussions on the
evolution of the mass function. 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2011
VL 732
IS 1
AR 33
DI 10.1088/0004-637X/732/1/33
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500033
ER
PT J
AU Chaplin, WJ
Kjeldsen, H
Bedding, TR
Christensen-Dalsgaard, J
Gilliland, RL
Kawaler, SD
Appourchaux, T
Elsworth, Y
Garcia, RA
Houdek, G
Karoff, C
Metcalfe, TS
Molenda-Zakowicz, J
Monteiro, MJPFG
Thompson, MJ
Verner, GA
Batalha, N
Borucki, WJ
Brown, TM
Bryson, ST
Christiansen, JL
Clarke, BD
Jenkins, JM
Klaus, TC
Koch, D
An, D
Ballot, J
Basu, S
Benomar, O
Bonanno, A
Broomhall, AM
Campante, TL
Corsaro, E
Creevey, OL
Esch, L
Gai, N
Gaulme, P
Hale, SJ
Handberg, R
Hekker, S
Huber, D
Mathur, S
Mosser, B
New, R
Pinsonneault, MH
Pricopi, D
Quirion, PO
Regulo, C
Roxburgh, IW
Salabert, D
Stello, D
Suran, MD
AF Chaplin, W. J.
Kjeldsen, H.
Bedding, T. R.
Christensen-Dalsgaard, J.
Gilliland, R. L.
Kawaler, S. D.
Appourchaux, T.
Elsworth, Y.
Garcia, R. A.
Houdek, G.
Karoff, C.
Metcalfe, T. S.
Molenda-Zakowicz, J.
Monteiro, M. J. P. F. G.
Thompson, M. J.
Verner, G. A.
Batalha, N.
Borucki, W. J.
Brown, T. M.
Bryson, S. T.
Christiansen, J. L.
Clarke, B. D.
Jenkins, J. M.
Klaus, T. C.
Koch, D.
An, D.
Ballot, J.
Basu, S.
Benomar, O.
Bonanno, A.
Broomhall, A. -M.
Campante, T. L.
Corsaro, E.
Creevey, O. L.
Esch, L.
Gai, N.
Gaulme, P.
Hale, S. J.
Handberg, R.
Hekker, S.
Huber, D.
Mathur, S.
Mosser, B.
New, R.
Pinsonneault, M. H.
Pricopi, D.
Quirion, P. -O.
Regulo, C.
Roxburgh, I. W.
Salabert, D.
Stello, D.
Suran, M. D.
TI PREDICTING THE DETECTABILITY OF OSCILLATIONS IN SOLAR-TYPE STARS
OBSERVED BY KEPLER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: interiors; stars: late-type; stars: oscillations
ID MAIN-SEQUENCE STARS; THEORETICAL ISOCHRONES; PHOTOMETRIC SYSTEMS; HR
DIAGRAM; ASTEROSEISMOLOGY; CONVECTION; MISSION; AMPLITUDES; PARAMETERS;
EVOLUTION
AB Asteroseismology of solar-type stars has an important part to play in the exoplanet program of the NASA Kepler Mission. Precise and accurate inferences on the stellar properties that are made possible by the seismic data allow very tight constraints to be placed on the exoplanetary systems. Here, we outline how to make an estimate of the detectability of solar-like oscillations in any given Kepler target, using rough estimates of the temperature and radius, and the Kepler apparent magnitude.
C1 [Chaplin, W. J.; Elsworth, Y.; Verner, G. A.; Broomhall, A. -M.; Hale, S. J.; Hekker, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Kjeldsen, H.; Christensen-Dalsgaard, J.; Karoff, C.; Campante, T. L.; Handberg, R.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark.
[Bedding, T. R.; Huber, D.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Appourchaux, T.; Benomar, O.; Gaulme, P.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France.
[Garcia, R. A.] Univ Paris Diderot, IRFU SAp, CNRS, CEA DSM,Lab AIM, F-91191 Gif Sur Yvette, France.
[Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Metcalfe, T. S.; Thompson, M. J.; Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Metcalfe, T. S.; Thompson, M. J.; Huber, D.] Natl Ctr Atmospher Res, Div Comp Sci, Boulder, CO 80307 USA.
[Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland.
[Monteiro, M. J. P. F. G.; Campante, T. L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Monteiro, M. J. P. F. G.; Campante, T. L.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
[Verner, G. A.; Roxburgh, I. W.] Univ London, Astron Unit, London E1 4NS, England.
[Christiansen, J. L.; Clarke, B. D.; Jenkins, J. M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Klaus, T. C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[An, D.] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
[Ballot, J.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Basu, S.; Esch, L.; Gai, N.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Bonanno, A.; Corsaro, E.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Creevey, O. L.; Regulo, C.; Salabert, D.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Creevey, O. L.; Regulo, C.; Salabert, D.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Gai, N.] Beijing Normal Univ, Beijing 100875, Peoples R China.
[Hekker, S.] Univ Amsterdam, Astron Inst, NL-1090 GE Amsterdam, Netherlands.
[Mosser, B.] Univ Paris 07, Univ Paris 06, Observ Paris, CNRS,LESIA, F-92195 Meudon, France.
[New, R.] Sheffield Hallam Univ, Mat Engn Res Inst, Fac Arts Comp Engn & Sci, Sheffield S1 1WB, S Yorkshire, England.
[Pinsonneault, M. H.] Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA.
[Pricopi, D.; Suran, M. D.] Acad Romana, Astron Inst, RO-40557 Bucharest, Romania.
[Quirion, P. -O.] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada.
RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
RI Ballot, Jerome/G-1019-2010; Monteiro, Mario J.P.F.G./B-4715-2008; Hale,
Steven/E-3472-2015;
OI Kawaler, Steven/0000-0002-6536-6367; Monteiro, Mario
J.P.F.G./0000-0003-0513-8116; Hale, Steven/0000-0002-6402-8382; Bonanno,
Alfio/0000-0003-3175-9776; 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
FU NASA's Science Mission Directorate; UK Science and Technology Facilities
Council (STFC); Netherlands Organisation for Scientific Research (NWO);
National Science Foundation; International Space Science Institute
(ISSI)
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors wish to thank the entire Kepler team, without
whom these results would not be possible. We also thank all funding
councils and agencies that have supported the activities of KASC Working
Group 1. W.J.C., Y.E., S.J.H., and G.A.V. acknowledge the support of the
UK Science and Technology Facilities Council (STFC). S.H. acknowledges
support from the Netherlands Organisation for Scientific Research (NWO).
NCAR is supported by the National Science Foundation. We are also
grateful for support from the International Space Science Institute
(ISSI).
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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 MAY 1
PY 2011
VL 732
IS 1
AR 54
DI 10.1088/0004-637X/732/1/54
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500054
ER
PT J
AU Cognard, I
Guillemot, L
Johnson, TJ
Smith, DA
Venter, C
Harding, AK
Wolff, MT
Cheung, CC
Donato, D
Abdo, AA
Ballet, J
Camilo, F
Desvignes, G
Dumora, D
Ferrara, EC
Freire, PCC
Grove, JE
Johnston, S
Keith, M
Kramer, M
Lyne, AG
Michelson, PF
Parent, D
Ransom, SM
Ray, PS
Romani, RW
Parkinson, PMS
Stappers, BW
Theureau, G
Thompson, DJ
Weltevrede, P
Wood, KS
AF Cognard, I.
Guillemot, L.
Johnson, T. J.
Smith, D. A.
Venter, C.
Harding, A. K.
Wolff, M. T.
Cheung, C. C.
Donato, D.
Abdo, A. A.
Ballet, J.
Camilo, F.
Desvignes, G.
Dumora, D.
Ferrara, E. C.
Freire, P. C. C.
Grove, J. E.
Johnston, S.
Keith, M.
Kramer, M.
Lyne, A. G.
Michelson, P. F.
Parent, D.
Ransom, S. M.
Ray, P. S.
Romani, R. W.
Parkinson, P. M. Saz
Stappers, B. W.
Theureau, G.
Thompson, D. J.
Weltevrede, P.
Wood, K. S.
TI DISCOVERY OF TWO MILLISECOND PULSARS IN FERMI SOURCES WITH THE NANCAY
RADIO TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: general; pulsars: general; pulsars: individual (J2017+0603,
J2302+4442)
ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; LIGHT CURVES; MONTE-CARLO;
EMISSION; CATALOG; POPULATION; BINARY; RADIATION; TUCANAE
AB We report the discovery of two millisecond pulsars in a search for radio pulsations at the positions of Fermi-Large Area Telescope sources with no previously known counterparts, using the Nancay Radio Telescope. The two millisecond pulsars, PSRs J2017+0603 and J2302+4442, have rotational periods of 2.896 and 5.192 ms and are both in binary systems with low-eccentricity orbits and orbital periods of 2.2 and 125.9 days, respectively, suggesting long recycling processes. Gamma-ray pulsations were subsequently detected for both objects, indicating that they power the associated Fermi sources in which they were found. The gamma-ray light curves and spectral properties are similar to those of previously detected gamma-ray millisecond pulsars. Detailed modeling of the observed radio and gamma-ray light curves shows that the gamma-ray emission seems to originate at high altitudes in their magnetospheres. Additionally, X-ray observations revealed the presence of an X-ray source at the position of PSR J2302+4442, consistent with thermal emission from a neutron star. These discoveries along with the numerous detections of radio-loud millisecond pulsars in gamma rays suggest that many Fermi sources with no known counterpart could be unknown millisecond pulsars.
C1 [Cognard, I.; Theureau, G.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 02, France.
[Cognard, I.; Theureau, G.] Observ Paris, CNRS, INSU, Stn Radioastron Nancay, F-18330 Nancay, France.
[Guillemot, L.; Freire, P. C. C.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Johnson, T. J.; Harding, A. K.; Ferrara, E. C.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Johnson, T. J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Johnson, T. J.; Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Smith, D. A.; Dumora, D.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucleaires Bordeaux Gradignan, F-33175 Gradignan, France.
[Venter, C.] North West Univ, ZA-2520 Potchefstroom, South Africa.
[Wolff, M. T.; Grove, J. E.; Ray, P. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Cheung, C. C.; Abdo, A. A.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Donato, D.] CRESST, Greenbelt, MD 20771 USA.
[Donato, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ballet, J.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Desvignes, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Desvignes, G.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Johnston, S.; Keith, M.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Kramer, M.; Lyne, A. G.; Stappers, B. W.; Weltevrede, P.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Michelson, P. F.; Romani, R. W.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Michelson, P. F.; Romani, R. W.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Parent, D.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RP Cognard, I (reprint author), Univ Orleans, CNRS, LPC2E, F-45071 Orleans 02, France.
EM icognard@cnrs-orleans.fr; guillemo@mpifr-bonn.mpg.de;
tyrel.j.johnson@gmail.com
RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Venter,
Christo/E-6884-2011;
OI Thompson, David/0000-0001-5217-9135; Venter,
Christo/0000-0002-2666-4812; Ransom, Scott/0000-0001-5799-9714; Ray,
Paul/0000-0002-5297-5278
FU Science and Technology Facilities Council of the United Kingdom
FX The Nancay Radio Observatory is operated by the Paris Observatory,
associated with the French Centre National de la Recherche Scientifique.
The Green Bank Telescope is operated by the National Radio Astronomy
Observatory, a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. The Lovell
Telescope is owned and operated by the University of Manchester as part
of the Jodrell Bank Centre for Astrophysics with support from the
Science and Technology Facilities Council of the United Kingdom.
NR 63
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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 MAY 1
PY 2011
VL 732
IS 1
AR 47
DI 10.1088/0004-637X/732/1/47
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500047
ER
PT J
AU Currie, T
Sicilia-Aguilar, A
AF Currie, Thayne
Sicilia-Aguilar, Aurora
TI THE TRANSITIONAL PROTOPLANETARY DISK FREQUENCY AS A FUNCTION OF AGE:
DISK EVOLUTION IN THE CORONET CLUSTER, TAURUS, AND OTHER 1-8 Myr OLD
REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: formation; protoplanetary disks; stars: pre-main
sequence
ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS;
SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; LOW-MASS STARS;
2-DIMENSIONAL RADIATIVE-TRANSFER; ETA CHAMAELEONTIS CLUSTER;
CIRCUMSTELLAR DUST DISKS; DEBRIS DISKS; PLANET FORMATION
AB We present Spitzer 3.6-24 mu m photometry and spectroscopy for stars in the 1-3 Myr old Coronet Cluster, expanding upon the survey of Sicilia-Aguilar et al. Using sophisticated radiative transfer models, we analyze these new data and those from Sicilia-Aguilar et al. to identify disks with evidence for substantial dust evolution consistent with disk clearing: transitional disks. We then analyze data in Taurus and others young clusters-IC 348, NGC 2362, and eta Cha-to constrain the transitional disk frequency as a function of time. Our analysis confirms previous results finding evidence for two types of transitional disks-those with inner holes and those that are homologously depleted. The percentage of disks in the transitional phase increases from similar to 15%-20% at 1-2 Myr to >= 50% at 5-8 Myr; the mean transitional disk lifetime is closer to similar to 1 Myr than 0.1-0.5 Myr, consistent with previous studies by Currie et al. and Sicilia-Aguilar et al. In the Coronet Cluster and IC 348, transitional disks are more numerous for very low mass M3-M6 stars than for more massive K5-M2 stars, while Taurus lacks a strong spectral-type-dependent frequency. Assuming standard values for the gas-to-dust ratio and other disk properties, the lower limit for the masses of optically thick primordial disks is M-disk approximate to 0.001-0.003 M-star. We find that single color-color diagrams do not by themselves uniquely identify transitional disks or primordial disks. Full spectral energy distribution modeling is required to accurately assess disk evolution for individual sources and inform statistical estimates of the transitional disk population in large samples using mid-IR colors.
C1 [Currie, Thayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sicilia-Aguilar, Aurora] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Currie, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
FU NASA; Deutsche Forschungsgemeinschaft (DFG) [SI-1486/1-1]
FX The anonymous referee provided comments and suggestions that greatly
improved the organization and content of this paper. We thank Cornelis
Dullemond, Thomas Henning, Scott Kenyon, James Muzerolle, Carol Grady,
Adam Kraus, and Meredith Hughes for useful conversations and
suggestions. We also thank Richard Alexander for providing us with
output from his disk evolution models presented in Alexander & Armitage
(2009). Finally, we thank Jeroen Bouwman for assistance with our IRS
data reduction. T.C. is supported by a NASA Postdoctoral Fellowship;
A.S-A. acknowledges support from the Deutsche Forschungsgemeinschaft
(DFG) grant SI-1486/1-1. This work made extensive use of the SIMBAD
Astronomical Database.
NR 122
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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 MAY 1
PY 2011
VL 732
IS 1
AR 24
DI 10.1088/0004-637X/732/1/24
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500024
ER
PT J
AU Kashlinsky, A
Atrio-Barandela, F
Ebeling, H
AF Kashlinsky, A.
Atrio-Barandela, F.
Ebeling, H.
TI MEASURING THE DARK FLOW WITH PUBLIC X-RAY CLUSTER DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; early universe;
inflation; large-scale structure of universe
ID SCALE PECULIAR VELOCITIES; LOCAL GROUP; MILKY-WAY; GALAXIES; ANISOTROPY;
SAMPLE; SPECTROSCOPY; PHOTOMETRY; CATALOG; SEARCH
AB We present new results on the "dark flow" from a measurement of the dipole in the distribution of peculiar velocities of galaxy clusters, applying the methodology proposed and developed by us earlier. Our latest measurement is conducted using new, low-noise 7 yr WMAP data as well as an all-sky sample of X-ray-selected galaxy clusters compiled exclusively from published catalogs. Our analysis of the cosmic microwave background signature of the kinematic Sunyaev-Zel'dovich (SZ) effect finds a statistically significant dipole at the location of galaxy clusters. The residual dipole outside the cluster regions is small, rendering our overall measurement 3s-4s significant. The amplitude of the dipole correlates with cluster properties, being larger for the most X-ray luminous clusters, as required if the signal is produced by the SZ effect. Since it is measured at zero monopole, the dipole cannot be due to the thermal SZ effect. Our results are consistent with those obtained earlier by us from 5 yr WMAP data and using a proprietary cluster catalog. In addition, they are robust to quadrupole removal, demonstrating that quadrupole leakage contributes negligibly to the signal. The lower noise of the 7 yr WMAP also allows us, for the first time, to obtain tentative empirical confirmation of our earlier conjecture that the adopted filtering alters the sign of the kinematic SZ (KSZ) effect for realistic clusters and thus of the deduced direction of the flow. The latter is consistent with our earlier measurement in both the amplitude and direction. Assuming the filtering indeed alters the sign of the KSZ effect from the clusters, the direction agrees well also with the results of independent work using galaxies as tracers at lower distances. We make all maps and cluster templates derived by us from public data available to the scientific community to allow independent tests of our method and findings.
C1 [Kashlinsky, A.] Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA.
[Kashlinsky, A.] Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Atrio-Barandela, F.] Univ Salamanca, E-37008 Salamanca, Spain.
[Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Kashlinsky, A (reprint author), Goddard Space Flight Ctr, SSAI, Code 665, Greenbelt, MD 20771 USA.
EM alexander.kashlinsky@nasa.gov
RI Atrio-Barandela, Fernando/A-7379-2017
OI Atrio-Barandela, Fernando/0000-0002-2130-2513
FU Spanish Ministerio de Educacion y Ciencia/Junta de Castilla y Leon
[NNG04G089G/09-ADP09-0050, FIS2009-07238/GR-234/SyEC CSD 2007-00050]
FX We acknowledge NASA NNG04G089G/09-ADP09-0050 and
FIS2009-07238/GR-234/SyEC CSD 2007-00050 grants from Spanish Ministerio
de Educacion y Ciencia/Junta de Castilla y Leon. We thank our
collaborators on the SCOUT/"dark flow" project, Dale Kocevski and
Alastair Edge, for their numerous valuable contributions to the project.
NR 36
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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 MAY 1
PY 2011
VL 732
IS 1
AR 1
DI 10.1088/0004-637X/732/1/1
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500001
ER
PT J
AU Minton, DA
Malhotra, R
AF Minton, David A.
Malhotra, Renu
TI SECULAR RESONANCE SWEEPING OF THE MAIN ASTEROID BELT DURING PLANET
MIGRATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; minor planets, asteroids: general; planets and
satellites: dynamical evolution and stability
ID LATE HEAVY BOMBARDMENT; SOLAR-SYSTEM; ORBITAL EVOLUTION; KUIPER-BELT;
ORIGIN; NEPTUNE; SIMULATIONS; CONSTRAINTS; IMPACTORS; NEBULA
AB We calculate the eccentricity excitation of asteroids produced by the sweeping nu(6) secular resonance during the epoch of planetesimal-driven giant planet migration in the early history of the solar system. We derive analytical expressions for the magnitude of the eccentricity change and its dependence on the sweep rate and on planetary parameters; the nu(6) sweeping leads to either an increase or a decrease of eccentricity depending on an asteroid's initial orbit. Based on the slowest rate of nu(6) sweeping that allows a remnant asteroid belt to survive, we derive a lower limit on Saturn's migration speed of similar to 0.15 AU Myr(-1) during the era that the nu(6) resonance swept through the inner asteroid belt (semimajor axis range 2.1-2.8 AU). This rate limit is for Saturn's current eccentricity and scales with the square of its eccentricity; the limit on Saturn's migration rate could be lower if its eccentricity were lower during its migration. Applied to an ensemble of fictitious asteroids, our calculations show that a prior single-peaked distribution of asteroid eccentricities would be transformed into a double-peaked distribution due to the sweeping of the nu(6) resonance. Examination of the orbital data of main belt asteroids reveals that the proper eccentricities of the known bright (H <= 10.8) asteroids may be consistent with a double-peaked distribution. If so, our theoretical analysis then yields two possible solutions for the migration rate of Saturn and for the dynamical states of the pre-migration asteroid belt: a dynamically cold state (single-peaked eccentricity distribution with mean of similar to 0.05) linked with Saturn'smigration speed similar to 4 AU Myr(-1) or a dynamically hot state (single-peaked eccentricity distribution with mean of similar to 0.3) linked with Saturn's migration speed similar to 0.8 AU Myr(-1).
C1 [Minton, David A.] SW Res Inst, Boulder, CO 80302 USA.
[Minton, David A.] NASA, Lunar Sci Inst, Boulder, CO 80302 USA.
[Malhotra, Renu] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
RP Minton, DA (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM daminton@boulder.swri.edu; renu@lpl.arizona.edu
OI Malhotra, Renu/0000-0002-1226-3305
FU NSF [AST-0806828]; NASA:NESSF [NNX08AW25H]; NASA NLSI/CLOE [NNA09DB32A]
FX The authors thank the anonymous reviewer and the editor Eric Feigelson
for useful comments. This research was supported in part by NSF grant
no. AST-0806828 and NASA:NESSF grant no. NNX08AW25H. The work of David
Minton was additionally partially supported by NASA NLSI/CLOE research
grant no. NNA09DB32A
NR 42
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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 MAY 1
PY 2011
VL 732
IS 1
AR 53
DI 10.1088/0004-637X/732/1/53
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500053
ER
PT J
AU Muchovej, S
Leitch, E
Carlstrom, JE
Culverhouse, T
Greer, C
Hawkins, D
Hennessy, R
Joy, M
Lamb, J
Loh, M
Marrone, DP
Miller, A
Mroczkowski, T
Pryke, C
Sharp, M
Woody, D
AF Muchovej, Stephen
Leitch, Erik
Carlstrom, John E.
Culverhouse, Thomas
Greer, Chris
Hawkins, David
Hennessy, Ryan
Joy, Marshall
Lamb, James
Loh, Michael
Marrone, Daniel P.
Miller, Amber
Mroczkowski, Tony
Pryke, Clem
Sharp, Matthew
Woody, David
TI COSMOLOGICAL CONSTRAINTS FROM A 31 GHz SKY SURVEY WITH THE
SUNYAEV-ZEL'DOVICH ARRAY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: general; large-scale structure of universe; surveys;
techniques: interferometric
ID SOUTH-POLE TELESCOPE; GALAXY CLUSTERS; POWER SPECTRUM; RADIO-SOURCES;
ANISOTROPY; REDSHIFT; PROBE; PARAMETERS; PRECISION; UNIVERSE
AB We present the results of an analysis of 4.4 deg(2) selected from a 6.1 deg(2) survey for clusters of galaxies via their Sunyaev-Zel'dovich effect at 31 GHz. From late 2005 to mid 2007, the Sunyaev-Zel'dovich Array observed four fields of roughly 1.5 deg(2) each. One of the fields shows evidence for significant diffuse Galactic emission, and is therefore excised from this analysis. We estimate the cluster detectability for the survey using mock observations of simulations of clusters of galaxies and determine that, at intermediate redshifts (z similar to 0.8), the survey is 50% complete to a limiting mass (M-200 (rho) over bar) of similar to 6.0 x 10(14) M-circle dot, with the mass limit decreasing at higher redshifts. We detect no clusters at a significance greater than five times the rms noise level in the maps, and place an upper limit on sigma(8), the amplitude of mass density fluctuations on a scale of 8 h(-1) Mpc, of 0.84 + 0.04 + 0.04 at 95% confidence, where the first uncertainty reflects an estimate of additional sample variance due to non-Gaussianity in the distribution of clusters and the second reflects calibration and systematic effects. This result is consistent with estimates from other cluster surveys and cosmic microwave background anisotropy experiments.
C1 [Muchovej, Stephen; Hawkins, David; Lamb, James; Woody, David] Owens Valley Radio Observ, CALTECH, Big Pine, CA 93513 USA.
[Muchovej, Stephen; Mroczkowski, Tony] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Leitch, Erik; Carlstrom, John E.; Culverhouse, Thomas; Greer, Chris; Hennessy, Ryan; Loh, Michael; Marrone, Daniel P.; Pryke, Clem; Sharp, Matthew] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Carlstrom, John E.] Univ Chicago, Dept Phys, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Joy, Marshall] NASA, Marshall Space Flight Ctr, Space Sci VP62, Huntsville, AL 35812 USA.
[Miller, Amber] Columbia Univ, Columbia Astrophys Lab, Dept Phys, New York, NY 10027 USA.
[Mroczkowski, Tony] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
RP Muchovej, S (reprint author), Owens Valley Radio Observ, CALTECH, Big Pine, CA 93513 USA.
OI Marrone, Daniel/0000-0002-2367-1080; Mroczkowski,
Tony/0000-0003-3816-5372
FU James S. McDonnell Foundation; National Science Foundation [AST-0507545,
AST-05-07161]; University of Chicago; NSF Division of Astronomical
Sciences [AST-0604982]; NSF Physics Frontier Center [PHY-0114422]; NASA
[HST-HF-51259.01]
FX We thank John Cartwright, Ben Reddall, and Marcus Runyan for their
significant contributions to the construction and commissioning of the
SZA instrument. We thank the staff of the Owens Valley Radio Observatory
and CARMA for their outstanding support. We thank Bryan Butler and Mark
Gurwell for providing the Mars model to which the SZA data are
calibrated. We also thank Laurie Shaw and Martin White for providing us
with the simulations used in this work. We gratefully acknowledge the
James S. McDonnell Foundation, the National Science Foundation, and the
University of Chicago for funding to construct the SZA. The operation of
the SZA is supported by NSF Division of Astronomical Sciences through
grant AST-0604982. Partial support is provided by NSF Physics Frontier
Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics
at the University of Chicago, and by NSF grants AST-0507545 and
AST-05-07161 to Columbia University. A. M. acknowledges support from a
Sloan Fellowship, D. P. M. from a Hubble Fellowship under NASA grant
HST-HF-51259.01, S. M. from an NSF Astronomy and Astrophysics
Fellowship, and C. G., S. M., and M. S. from NSF Graduate Research
Fellowships.
NR 40
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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 MAY 1
PY 2011
VL 732
IS 1
AR 28
DI 10.1088/0004-637X/732/1/28
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500028
ER
PT J
AU Raichoor, A
Mei, S
Nakata, F
Stanford, SA
Holden, BP
Rettura, A
Huertas-Company, M
Postman, M
Rosati, P
Blakeslee, JP
Demarco, R
Eisenhardt, P
Illingworth, G
Jee, MJ
Kodama, T
Tanaka, M
White, RL
AF Raichoor, A.
Mei, S.
Nakata, F.
Stanford, S. A.
Holden, B. P.
Rettura, A.
Huertas-Company, M.
Postman, M.
Rosati, P.
Blakeslee, J. P.
Demarco, R.
Eisenhardt, P.
Illingworth, G.
Jee, M. J.
Kodama, T.
Tanaka, M.
White, R. L.
TI EARLY-TYPE GALAXIES AT z similar to 1.3. II. MASSES AND AGES OF
EARLY-TYPE GALAXIES IN DIFFERENT ENVIRONMENTS AND THEIR DEPENDENCE ON
STELLAR POPULATION MODEL ASSUMPTIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (RX J0849+4452, RX J0848+4453); galaxies:
elliptical and lenticular, cD; galaxies: evolution; galaxies: formation;
galaxies: high-redshift; galaxies: photometry
ID HIGH-REDSHIFT GALAXIES; COLOR-MAGNITUDE RELATION; GIANT BRANCH STARS;
DIGITAL SKY SURVEY; GOODS-SOUTH FIELD; VLT DEEP SURVEY; TP-AGB STARS;
LUMINOSITY FUNCTION; LYNX SUPERCLUSTER; PASSIVE GALAXIES
AB We have derived masses and ages for 79 early-type galaxies (ETGs) in different environments at z similar to 1.3 in the Lynx supercluster and in the GOODS/CDF-S field using multi-wavelength (0.6-4.5 mu m; KPNO, Palomar, Keck, Hubble Space Telescope, Spitzer) data sets. At this redshift the contribution of the thermally pulsing asymptotic giant branch (TP-AGB) phase is important for ETGs, and the mass and age estimates depend on the choice of the stellar population model used in the spectral energy distribution fits. We describe in detail the differences among model predictions for a large range of galaxy ages, showing the dependence of these differences on age. Current models still yield large uncertainties. While recent models from Maraston and Charlot & Bruzual offer better modeling of the TP-AGB phase with respect to less recent Bruzual & Charlot models, their predictions do not often match. The modeling of this TP-AGB phase has a significant impact on the derived parameters for galaxies observed at high redshift. Some of our results do not depend on the choice of the model: for all models, the most massive galaxies are the oldest ones, independent of the environment. When using the Maraston and Charlot & Bruzual models, the mass distribution is similar in the clusters and in the groups, whereas in our field sample there is a deficit of massive (M greater than or similar to 10(11) M-circle dot) ETGs. According to those last models, ETGs belonging to the cluster environment host on average older stars with respect to group and field populations. This difference is less significant than the age difference in galaxies of different masses.
C1 [Raichoor, A.; Mei, S.; Huertas-Company, M.] Observ Paris, Sect Meudon, GEPI, F-92190 Meudon, France.
[Mei, S.; Huertas-Company, M.] Univ Paris Denis Diderot, F-75205 Paris 13, France.
[Mei, S.] CALTECH, Pasadena, CA 91125 USA.
[Nakata, F.; Kodama, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Stanford, S. A.; Rettura, A.; Jee, M. J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA.
[Holden, B. P.; Illingworth, G.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95065 USA.
[Rettura, A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Postman, M.; White, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Rosati, P.] European S Observ, D-85748 Garching, Germany.
[Blakeslee, J. P.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Demarco, R.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kodama, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Tanaka, M.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
RP Raichoor, A (reprint author), Osserv Astron Brera, Via Brera 28, I-20121 Milan, Italy.
EM anand.raichoor@brera.inaf.it
OI Blakeslee, John/0000-0002-5213-3548
FU NASA [NAS 5-32865, NAS5-26555]; NASA HST [GO-10574.01-A]; Spitzer
[20694]; W. M. Keck Foundation
FX ACS was developed under NASA contract NAS 5-32865. This research has
been supported by the NASA HST grant GO-10574.01-A, and Spitzer grant
for program 20694. The Space Telescope Science Institute is operated by
AURA Inc., under NASA contract NAS5-26555. Some of the data presented
herein were obtained at the W. M. Keck Observatory, which is operated as
a scientific partnership among the California Institute of Technology,
the University of California and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous
financial support of the W. M. Keck Foundation. The authors recognize
and acknowledge the very significant cultural role and reverence that
the summit of Mauna Kea has always had within the indigenous Hawaiian
community. We are most fortunate to have the opportunity to conduct
observations from this mountain. Some data were based on observations
obtained at the Gemini Observatory, which is operated by the Association
of Universities for Research in Astronomy, Inc., under a cooperative
agreement with the NSF on behalf of the Gemini partnership: the National
Science Foundation (United States), the Science and Technology
Facilities Council (United Kingdom), the National Research Council
(Canada), CONlCYT (Chile), the Australian Research Council (Australia),
Ministrio da Cincia e Tecnologia (Brazil) and Ministerio de Ciencia,
Tecnologa e Innovacin Productiva (Argentina), Gemini Science Program ID:
GN-2006A-Q-78. We thank the anonymous referee for constructive comments.
We thank Raphael Gobat and Veronica Strazzullo for useful discussions.
NR 85
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2011
VL 732
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DI 10.1088/0004-637X/732/1/12
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500012
ER
PT J
AU Rigby, JR
Wuyts, E
Gladders, MD
Sharon, K
Becker, GD
AF Rigby, J. R.
Wuyts, E.
Gladders, M. D.
Sharon, K.
Becker, G. D.
TI THE PHYSICAL CONDITIONS OF A LENSED STAR-FORMING GALAXY AT z=1.7
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: evolution; galaxies: high-redshift;
gravitational lensing: strong
ID LYMAN BREAK GALAXY; MASS-METALLICITY RELATION; SIMILAR-TO 2; DIGITAL SKY
SURVEY; H-II REGIONS; MS 1512-CB58; HII-REGIONS; ULTRAVIOLET-SPECTRUM;
CHEMICAL-COMPOSITION; STELLAR POPULATIONS
AB We report rest-frame optical Keck/NIRSPEC spectroscopy of the bright lensed galaxy RCSGA 032727-132609 at z = 1.7037. From precise measurements of the nebular lines, we infer a number of physical properties: redshift, extinction, star formation rate, ionization parameter, electron density, electron temperature, oxygen abundance, and N/O, Ne/O, and Ar/O abundance ratios. The limit on [O III] 4363 angstrom tightly constrains the oxygen abundance via the "direct" or T-e method, for the first time in an average-metallicity galaxy at z similar to 2. We compare this result to several standard "bright-line" O abundance diagnostics, thereby testing these empirically-calibrated diagnostics in situ. Finally, we explore the positions of lensed and unlensed galaxies in standard diagnostic diagrams, and the diversity of ionization conditions and mass-metallicity ratios at z = 2.
C1 [Rigby, J. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wuyts, E.; Gladders, M. D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Wuyts, E.; Gladders, M. D.; Sharon, K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Becker, G. D.] Kavli Inst Cosmol, Cambridge, England.
[Rigby, J. R.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
RP Rigby, JR (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM Jane.R.Rigby@nasa.gov
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU Carnegie Fellowship; W.M. Keck Foundation
FX We thank the IRTF Spex team for making public their telluric correction
routine and their tool to find telluric standard stars, at
http://irtfweb.ifa.hawaii.edu/similar to spex/. We thank Kevin
Schawinski for code to generate the SDSS contours in Figure 7, which is
adapted from Schawinski et al. (2010); we thank Fuyan Bian for code to
generate Figure 6, which is adapted from Bian et al. (2010). We thank
Andrew Marble for use of his implementation of MPFITFUN (Markwardt 2009)
to fit multiple Gaussians. J.R.R. gratefully acknowledges the financial
support and intellectual freedom of a Carnegie Fellowship.; Data
presented herein were obtained at the W.M. Keck Observatory from
telescope time allocated to the National Aeronautics and Space
Administration through the agency's scientific partnership with the
California Institute of Technology and the University of California. The
Observatory was made possible by the generous financial support of the
W.M. Keck Foundation. 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 67
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2011
VL 732
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DI 10.1088/0004-637X/732/1/59
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500059
ER
PT J
AU Searles, JM
Destree, JD
Snow, TP
Salama, F
York, DG
Dahlstrom, J
AF Searles, Justin M.
Destree, Joshua D.
Snow, Theodore P.
Salama, Farid
York, Donald G.
Dahlstrom, Julie
TI SEARCHING FOR NAPHTHALENE CATION ABSORPTION IN THE INTERSTELLAR MEDIUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: lines and bands; line: profiles; surveys
ID ANOMALOUS MICROWAVE EMISSION; PULSED DISCHARGE NOZZLE; RING-DOWN
SPECTROSCOPY; BANDS
AB Interstellar naphthalene cations (C10H8+) have been proposed by a study to be the carriers of a small number of diffuse interstellar bands (DIBs). Using an archive of high signal-to-noise spectra obtained at the Apache Point Observatory, we used two methods to test the hypothesis. Both methods failed to detect significant absorption at lab wavelengths of interstellar spectra with laboratory spectra. We thereby conclude that C10H8+ is not a DIB carrier in typical reddened sight lines.
C1 [Searles, Justin M.; Destree, Joshua D.; Snow, Theodore P.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Salama, Farid] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Dahlstrom, Julie] Carthage Coll, Kenosha, WI 53140 USA.
RP Searles, JM (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Campus Box 391, Boulder, CO 80309 USA.
EM searlesj@colorado.edu; destree@colorado.edu; tsnow@casa.colorado.edu;
Farid.Salama@nasa.gov; don@oddjob.uchicago.edu; jdahlstrom1@carthage.edu
RI Salama, Farid/A-8787-2009
OI Salama, Farid/0000-0002-6064-4401
FU NASA [NNX08AC14G]
FX This research was supported by NASA grant NNX08AC14G.
NR 24
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2011
VL 732
IS 1
AR 50
DI 10.1088/0004-637X/732/1/50
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500050
ER
PT J
AU Sehgal, N
Trac, H
Acquaviva, V
Ade, PAR
Aguirre, P
Amiri, M
Appel, JW
Barrientos, LF
Battistelli, ES
Bond, JR
Brown, B
Burger, B
Chervenak, J
Das, S
Devlin, MJ
Dicker, SR
Doriese, WB
Dunkley, J
Dunner, R
Essinger-Hileman, T
Fisher, RP
Fowler, JW
Hajian, A
Halpern, M
Hasselfield, M
Hernandez-Monteagudo, C
Hilton, GC
Hilton, M
Hincks, AD
Hlozek, R
Holtz, D
Huffenberger, KM
Hughes, DH
Hughes, JP
Infante, L
Irwin, KD
Jones, A
Juin, JB
Klein, J
Kosowsky, A
Lau, JM
Limon, M
Lin, YT
Lupton, RH
Marriage, TA
Marsden, D
Martocci, K
Mauskopf, P
Menanteau, F
Moodley, K
Moseley, H
Netterfield, CB
Niemack, MD
Nolta, MR
Page, LA
Parker, L
Partridge, B
Reid, B
Sherwin, BD
Sievers, J
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Tucker, C
Warne, R
Wollack, E
Zhao, Y
AF Sehgal, Neelima
Trac, Hy
Acquaviva, Viviana
Ade, Peter A. R.
Aguirre, Paula
Amiri, Mandana
Appel, John W.
Felipe Barrientos, L.
Battistelli, Elia S.
Bond, J. Richard
Brown, Ben
Burger, Bryce
Chervenak, Jay
Das, Sudeep
Devlin, Mark J.
Dicker, Simon R.
Doriese, W. Bertrand
Dunkley, Joanna
Duenner, Rolando
Essinger-Hileman, Thomas
Fisher, Ryan P.
Fowler, Joseph W.
Hajian, Amir
Halpern, Mark
Hasselfield, Matthew
Hernandez-Monteagudo, Carlos
Hilton, Gene C.
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Holtz, David
Huffenberger, Kevin M.
Hughes, David H.
Hughes, John P.
Infante, Leopoldo
Irwin, Kent D.
Jones, Andrew
Baptiste Juin, Jean
Klein, Jeff
Kosowsky, Arthur
Lau, Judy M.
Limon, Michele
Lin, Yen-Ting
Lupton, Robert H.
Marriage, Tobias A.
Marsden, Danica
Martocci, Krista
Mauskopf, Phil
Menanteau, Felipe
Moodley, Kavilan
Moseley, Harvey
Netterfield, Calvin B.
Niemack, Michael D.
Nolta, Michael R.
Page, Lyman A.
Parker, Lucas
Partridge, Bruce
Reid, Beth
Sherwin, Blake D.
Sievers, Jon
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Thornton, Robert
Tucker, Carole
Warne, Ryan
Wollack, Ed
Zhao, Yue
TI THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED
VIA THE SUNYAEV-ZEL'DOVICH EFFECT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: general
ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; BACKGROUND POWER SPECTRUM;
TREE PARTICLE-MESH; X-RAY; RADIO-SOURCES; HYDRODYNAMICAL SIMULATIONS;
PECULIAR VELOCITIES; SCALING RELATIONS; CATALOG
AB We present constraints on cosmological parameters based on a sample of Sunyaev-Zel'dovich-selected (SZ-selected) galaxy clusters detected in a millimeter-wave survey by the Atacama Cosmology Telescope. The cluster sample used in this analysis consists of nine optically confirmed high-mass clusters comprising the high-significance end of the total cluster sample identified in 455 deg(2) of sky surveyed during 2008 at 148 GHz. We focus on the most massive systems to reduce the degeneracy between unknown cluster astrophysics and cosmology derived from SZ surveys. We describe the scaling relation between cluster mass and SZ signal with a four-parameter fit. Marginalizing over the values of the parameters in this fit with conservative priors gives sigma(8) = 0.851 +/- 0.115 and omega = -1.14 +/- 0.35 for a spatially flat wCDM cosmological model with Wilkinson Microwave Anisotropy Probe (WMAP) seven-year priors on cosmological parameters. This gives a modest improvement in statistical uncertainty over WMAP seven-year constraints alone. Fixing the scaling relation between the cluster mass and SZ signal to a fiducial relation obtained from numerical simulations and calibrated by X-ray observations, we find sigma(8) = 0.821 +/- 0.044 and omega = -1.05 +/- 0.20. These results are consistent with constraints from WMAP7 plus baryon acoustic oscillations plus Type Ia supernova which give sigma(8) = 0.802 +/- 0.038 and omega = -0.98 +/- 0.053. A stacking analysis of the clusters in this sample compared to clusters simulated assuming the fiducial model also shows good agreement. These results suggest that, given the sample of clusters used here, both the astrophysics of massive clusters and the cosmological parameters derived from them are broadly consistent with current models.
C1 [Sehgal, Neelima; Lau, Judy M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Acquaviva, Viviana; Das, Sudeep; Dunkley, Joanna; Hajian, Amir; Lin, Yen-Ting; Lupton, Robert H.; Marriage, Tobias A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Acquaviva, Viviana; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aguirre, Paula; Felipe Barrientos, L.; Duenner, Rolando; Infante, Leopoldo; Baptiste Juin, Jean; Lin, Yen-Ting] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Appel, John W.; Das, Sudeep; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Holtz, David; Jones, Andrew; Lau, Judy M.; Limon, Michele; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Bond, J. Richard; Hajian, Amir; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Chervenak, Jay; Moseley, Harvey; Wollack, Ed; Zhao, Yue] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Limon, Michele; Marriage, Tobias A.; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Doriese, W. Bertrand; Fowler, Joseph W.; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa.
[Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa.
[Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Hughes, David H.] INAOE, Puebla, Mexico.
[Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
[Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Martocci, Krista; Switzer, Eric R.] Kavli Inst Cosmol Phys, Lab Astrophys & Space Res, Chicago, IL 60637 USA.
[Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Reid, Beth] Univ Barcelona, ICC, E-08028 Barcelona, Spain.
[Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
RP Sehgal, N (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew
James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Huffenberger, Kevin/0000-0001-7109-0099; Menanteau,
Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074;
/0000-0002-0896-8628; Limon, Michele/0000-0002-5900-2698
FU US National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768]; Princeton University; University of Pennsylvania; Canada
Foundation for Innovation; Compute Canada; Government of Ontario;
Ontario Research Fund-Research Excellence; University of Toronto; U.S.
Department of Energy [DE-AC3-76SF00515]; NASA [NNX08AH30G]; Natural
Science and Engineering Research Council of Canada (NSERC); NSF Physics
Frontier Center [PHY-0114422]; FONDAP Centro de Astrofisica; RCUK; South
African National Research Foundation (NRF); Meraka Institute; South
African Square Kilometer Array (SKA) Project; CONICYT; MECESUP;
Fundacion Andes; Rhodes Trust; Berkeley Center for Cosmological Physics;
World Premier International Research Center Initiative, MEXT, Japan;
NASA Office of Space Science; [NSFAST-0546035]; [AST-0606975]
FX This work was supported by the US National Science Foundation through
awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731,
and PIRE-0507768. Funding was also provided by Princeton University and
the University of Pennsylvania. The PIRE program made possible exchanges
between Chile, South Africa, Spain, and the US that enabled this
research program. Computations were performed on the GPC supercomputer
at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation
for Innovation under the auspices of Compute Canada, the Government of
Ontario, Ontario Research Fund-Research Excellence, and the University
of Toronto.; N.S. is supported by the U.S. Department of Energy contract
to SLAC No. DE-AC3-76SF00515. A. H., T. M., S. D., and V. A. were
supported through NASA grant NNX08AH30G. A. H. received additional
support from a Natural Science and Engineering Research Council of
Canada (NSERC) PGS-D scholarship. A. K. and B. P. were partially
supported through NSFAST-0546035 and AST-0606975, respectively, for work
on ACT. E. S. acknowledges support by NSF Physics Frontier Center grant
PHY-0114422 to the Kavli Institute of Cosmological Physics. H. Q. and L.
I. acknowledge partial support from FONDAP Centro de Astrofisica. J.D.
received support from an RCUK Fellowship. K. M., M. H., and R. W.
received financial support from the South African National Research
Foundation (NRF), the Meraka Institute via funding for the South African
Centre for High Performance Computing (CHPC), and the South African
Square Kilometer Array (SKA) Project. R. D. was supported by CONICYT,
MECESUP, and Fundacion Andes. RH acknowledges funding from the Rhodes
Trust. S. D. acknowledges support from the Berkeley Center for
Cosmological Physics. Y.T.L. acknowledges support from the World Premier
International Research Center Initiative, MEXT, Japan. 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. The data will be made
public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web
site (http://www.physics.princeton.edu/act/).
NR 87
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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 MAY 1
PY 2011
VL 732
IS 1
AR 44
DI 10.1088/0004-637X/732/1/44
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500044
ER
PT J
AU Stacey, WS
Heinke, CO
Elsner, RF
Edmonds, PD
Weisskopf, MC
Grindlay, JE
AF Stacey, W. S.
Heinke, C. O.
Elsner, R. F.
Edmonds, P. D.
Weisskopf, M. C.
Grindlay, J. E.
TI TRANSIENT EXTREMELY SOFT X-RAY EMISSION FROM THE UNUSUALLY BRIGHT
CATACLYSMIC VARIABLE IN THE GLOBULAR CLUSTER M3: A NEW CV X-RAY
LUMINOSITY RECORD?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; globular clusters: individual (NGC 5272);
novae, cataclysmic variables; white dwarfs; X-rays: binaries
ID ABSOLUTE MAGNITUDES; SUPERSOFT SOURCES; ACCRETION DISKS;
GALACTIC-CENTER; IA SUPERNOVAE; SKY SURVEY; GK-PERSEI; BINARIES;
EVOLUTION; NOVAE
AB We observed the accreting white dwarf (WD) 1E1339.8+2837 (1E1339) in the globular cluster M3 in 2003 November, 2004 May, and 2005 January, using the Chandra ACIS-S detector. The source was observed in 1992 to possess traits of a supersoft X-ray source (SSS), with a 0.1-2.4 keV luminosity as large as 2 x 10(35) erg s(-1), after which time the source's luminosity fell by roughly two orders of magnitude, adopting a hard X-ray spectrum more typical of cataclysmic variables (CVs). Our observations confirm 1E1339's hard CV-like spectrum, with photon index Gamma = 1.3 +/- 0.2. We found 1E1339 to be highly variable, with a 0.5-10 keV luminosity ranging from (1.4 +/- 0.3) x 10(34) erg s-1 to 8.5(-4.6)(+4.9) x 10(32) erg s(-1), with 1E1339's maximum luminosity being perhaps the highest yet recorded for hard X-ray emission from a WD. In 2005 January, 1E1339 displayed substantial low-energy emission below similar to 0.3 keV. Although current Chandra responses cannot properly model this emission, its bolometric luminosity appears comparable to or greater than that of the hard spectral component. This raises the possibility that the supersoft X-ray emission seen from 1E1339 in 1992 may have shifted to the far-UV.
C1 [Stacey, W. S.; Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Elsner, R. F.; Weisskopf, M. C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Edmonds, P. D.; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Stacey, WS (reprint author), Univ Alberta, Dept Phys, 11322-89 Ave, Edmonton, AB T6G 2G7, Canada.
EM heinke@ualberta.ca
OI Heinke, Craig/0000-0003-3944-6109
NR 44
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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 MAY 1
PY 2011
VL 732
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500046
ER
PT J
AU Vacca, WD
Sandell, G
AF Vacca, William D.
Sandell, Goeran
TI NEAR-INFRARED SPECTROSCOPY OF TW Hya: A REVISED SPECTRAL TYPE AND
COMPARISON WITH MAGNETOSPHERIC ACCRETION MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (TW Hya); stars: pre-main sequence; techniques:
spectroscopic
ID LOW-MASS STARS; RECOMBINATION-LINE-INTENSITIES; MAIN-SEQUENCE STARS;
TAURI STARS; HYDRAE ASSOCIATION; DISK ACCRETION; YOUNG STARS; TELESCOPE
FACILITY; CIRCUMSTELLAR DISK; HYDROGENIC IONS
AB We present high signal-to-noise ratio (S/N), moderate spectral resolution (R similar to 2000-2500) near-infrared (0.8-5.0 mu m) spectroscopy of the nearby T Tauri star TW Hya. By comparing the spectrum and the equivalent widths of several atomic and molecular features with those for stars in the IRTF near-infrared library, we revise the spectral type to M2.5V, which is later than what is usually adopted (K7V). This implies a substantially cooler stellar temperature than previously assumed. Comparison with various pre-main-sequence models suggests that TW Hya is only similar to 3 Myr old, much younger than the usually adopted 8-10 Myr. Analysis of the relative strengths of the H lines seen in the spectrum yields estimates for the temperature and density of the emitting region of T-e >= 7500 K and n(e) similar to 10(12)-10(13) cm(-3). The thickness of the emitting region is 10(2)-10(4) km and the covering fraction is f(*) similar to 0.04. Our derived physical parameter values agree with the predictions of the magnetospheric accretion scenario. The highest S/N H lines have profiles that indicate multiple emission components. We derive an excess spectrum (above that of the M2.5V template) that peaks in the H band. Although our derived veiling values (similar to 0.1) agree with previous estimates, the excess spectrum does not match that of current models in which this flux is generated by an inner optically thin disk. We suggest that the excess flux spectrum instead reflects the differences in atmospheric opacity, gravity, and age between TW Hya and older, higher gravity, field M2.5 dwarfs.
C1 [Vacca, William D.; Sandell, Goeran] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Vacca, WD (reprint author), NASA, SOFIA USRA, Ames Res Ctr, Mail Stop 211-3,Bldg N211,Rm 251, Moffett Field, CA 94035 USA.
EM wvacca@sofia.usra.edu; gsandell@sofia.usra.edu
FU National Aeronautics and Space Administration, Science Mission
Directorate [NNX-08AE38A]
FX Visiting Astronomer at the Infrared Telescope Facility, which is
operated by the University of Hawaii under Cooperative Agreement No.
NNX-08AE38A with the National Aeronautics and Space Administration,
Science Mission Directorate, Planetary Astronomy Program.
NR 79
TC 40
Z9 40
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2011
VL 732
IS 1
AR 8
DI 10.1088/0004-637X/732/1/8
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751OD
UT WOS:000289626500008
ER
PT J
AU Rosenzweig, C
Solecki, WD
Blake, R
Bowman, M
Faris, C
Gornitz, V
Horton, R
Jacob, K
LeBlanc, A
Leichenko, R
Linkin, M
Major, D
O'Grady, M
Patrick, L
Sussman, E
Yohe, G
Zimmerman, R
AF Rosenzweig, Cynthia
Solecki, William D.
Blake, Reginald
Bowman, Malcolm
Faris, Craig
Gornitz, Vivien
Horton, Radley
Jacob, Klaus
LeBlanc, Alice
Leichenko, Robin
Linkin, Megan
Major, David
O'Grady, Megan
Patrick, Lesley
Sussman, Edna
Yohe, Gary
Zimmerman, Rae
TI Developing coastal adaptation to climate change in the New York City
infrastructure-shed: process, approach, tools, and strategies
SO CLIMATIC CHANGE
LA English
DT Article
ID SEA-LEVEL RISE; IMPACTS; BOSTON
AB While current rates of sea level rise and associated coastal flooding in the New York City region appear to be manageable by stakeholders responsible for communications, energy, transportation, and water infrastructure, projections for sea level rise and associated flooding in the future, especially those associated with rapid icemelt of the Greenland and West Antarctic Icesheets, may be outside the range of current capacity because extreme events might cause flooding beyond today's planning and preparedness regimes. This paper describes the comprehensive process, approach, and tools for adaptation developed by the New York City Panel on Climate Change (NPCC) in conjunction with the region's stakeholders who manage its critical infrastructure, much of which lies near the coast. It presents the adaptation framework and the sea-level rise and storm projections related to coastal risks developed through the stakeholder process. Climate change adaptation planning in New York City is characterized by a multi-jurisdictional stakeholder-scientist process, state-of-the-art scientific projections and mapping, and development of adaptation strategies based on a risk-management approach.
C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Solecki, William D.; Patrick, Lesley] CUNY Hunter Coll, New York, NY 10021 USA.
[Blake, Reginald] CUNY, New York City Coll Technol, Brooklyn, NY 11210 USA.
[Bowman, Malcolm] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Faris, Craig] Accenture, Washington, DC USA.
[Gornitz, Vivien; Horton, Radley; Jacob, Klaus; Major, David; O'Grady, Megan] Columbia Univ, New York, NY USA.
[Leichenko, Robin] Rutgers State Univ, Piscataway, NJ USA.
[Linkin, Megan] Swiss Reinsurance Amer Corp, Armonk, NY USA.
[Sussman, Edna] Sussman ADR LLC, New York, NY USA.
[Yohe, Gary] Wesleyan Univ, Middletown, CT USA.
[Zimmerman, Rae] NYU, New York, NY USA.
RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM crosenzweig@giss.nasa.gov; aliceleblanc@verizon.net
RI Leichenko, Robin/C-6047-2013
OI Leichenko, Robin/0000-0003-0607-5874
NR 53
TC 54
Z9 54
U1 6
U2 67
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 MAY
PY 2011
VL 106
IS 1
SI SI
BP 93
EP 127
DI 10.1007/s10584-010-0002-8
PG 35
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 747CW
UT WOS:000289298900006
ER
PT J
AU Kim, H
Liou, MS
AF Kim, Hyoungjin
Liou, Meng-Sing
TI Accurate adaptive level set method and sharpening technique for three
dimensional deforming interfaces
SO COMPUTERS & FLUIDS
LA English
DT Article
DE Level set; Re-initialization; Interface tracking; Interface sharpening
ID INCOMPRESSIBLE 2-PHASE FLOWS; EFFICIENT IMPLEMENTATION; ALGORITHM;
SCHEMES
AB In this paper, we demonstrate improved accuracy of the level set method for resolving deforming interfaces by proposing two key elements: (1) accurate level set solutions on adapted Cartesian grids by judiciously choosing interpolation polynomials in regions of different grid levels and (2) enhanced re-initialization by an interface sharpening procedure. The level set equation is solved using a fifth order WENO scheme or a second order central differencing scheme depending on availability of uniform stencils at each grid point. Grid adaptation criteria are determined so that the Hamiltonian functions at nodes adjacent to interfaces are always calculated by the fifth order WENO scheme. This selective usage between the fifth order WENO and second order central differencing schemes is confirmed to give more accurate results compared to those in literature for standard test problems. In order to further improve accuracy especially near thin filaments, we suggest an artificial sharpening method, which is in a similar form with the conventional re-initialization method but utilizes sign of curvature instead of sign of the level set function. Consequently, volume loss due to numerical dissipation on thin filaments is remarkably reduced for the test problems. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Kim, Hyoungjin] NASA Glenn Res Ctr, NASA Postdoctoral Program, Cleveland, OH 44135 USA.
[Liou, Meng-Sing] NASA Glenn Res Ctr, Aeropropuls Div, Cleveland, OH 44135 USA.
RP Kim, H (reprint author), NASA Glenn Res Ctr, Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44135 USA.
EM hyoungjinkim1@gmail.com
FU Oak Ridge Associated Universities through a contract with NASA
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Glenn Research Center, administered by Oak Ridge
Associated Universities through a contract with NASA.
NR 20
TC 7
Z9 7
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-7930
EI 1879-0747
J9 COMPUT FLUIDS
JI Comput. Fluids
PD MAY
PY 2011
VL 44
IS 1
BP 111
EP 129
DI 10.1016/j.compfluid.2010.12.020
PG 19
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 747LG
UT WOS:000289320700011
ER
PT J
AU Bryson, S
Epshteyn, Y
Kurganov, A
Petrova, G
AF Bryson, Steve
Epshteyn, Yekaterina
Kurganov, Alexander
Petrova, Guergana
TI WELL-BALANCED POSITIVITY PRESERVING CENTRAL-UPWIND SCHEME ON TRIANGULAR
GRIDS FOR THE SAINT-VENANT SYSTEM
SO ESAIM-MATHEMATICAL MODELLING AND NUMERICAL ANALYSIS-MODELISATION
MATHEMATIQUE ET ANALYSE NUMERIQUE
LA English
DT Article
DE Hyperbolic systems of conservation and balance laws; semi-discrete
central-upwind schemes; Saint-Venant system of shallow water equations
ID HYPERBOLIC CONSERVATION-LAWS; SHALLOW-WATER EQUATIONS; FINITE-VOLUME
SCHEMES; UNSTRUCTURED GRIDS; SOURCE TERMS; WENO SCHEMES; ORDER; FLOWS;
ACCURACY; LIMITERS
AB We introduce a new second-order central-upwind scheme for the Saint-Venant system of shallow water equations on triangular grids. We prove that the scheme both preserves "lake at rest" steady states and guarantees the positivity of the computed fluid depth. Moreover, it can be applied to models with discontinuous bottom topography and irregular channel widths. We demonstrate these features of the new scheme, as well as its high resolution and robustness in a number of numerical examples.
C1 [Bryson, Steve] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Epshteyn, Yekaterina] Carnegie Mellon Univ, Dept Math Sci, Pittsburgh, PA 15213 USA.
[Kurganov, Alexander] Tulane Univ, Dept Math, New Orleans, LA 70118 USA.
[Petrova, Guergana] Texas A&M Univ, Dept Math, College Stn, TX 77843 USA.
RP Bryson, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Stephen.T.Bryson@nasa.gov; rina10@andrew.cmu.edu;
kurganov@math.tulane.edu; gpetrova@math.tamu.edu
RI Kurganov, Alexander/H-8789-2013
OI Kurganov, Alexander/0000-0003-0231-986X
FU Center for Nonlinear Analysis (CNA) under the NSF [DMS-0635983]; NSF
[DMS-0610430, DMS-0810869]; King Abdullah University of Science and
Technology (KAUST) [KUS-C1-016-04]
FX The research of Y. Epshteyn is based upon work supported by the Center
for Nonlinear Analysis (CNA) under the NSF Grant # DMS-0635983. The
research of A. Kurganov was supported in part by the NSF Grant #
DMS-0610430. The research of G. Petrova was supported in part by the NSF
Grant # DMS-0810869 and Award # KUS-C1-016-04, made by King Abdullah
University of Science and Technology (KAUST).
NR 37
TC 28
Z9 29
U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0764-583X
EI 1290-3841
J9 ESAIM-MATH MODEL NUM
JI ESAIM-Math. Model. Numer. Anal.-Model. Math. Anal. Numer.
PD MAY-JUN
PY 2011
VL 45
IS 3
BP 423
EP 446
DI 10.1051/m2an/2010060
PG 24
WC Mathematics, Applied
SC Mathematics
GA 751MS
UT WOS:000289622800002
ER
PT J
AU Holzmann, GJ
Florian, M
AF Holzmann, Gerard J.
Florian, Mihai
TI Model checking with bounded context switching
SO FORMAL ASPECTS OF COMPUTING
LA English
DT Article
DE Logic model checking; Depth-first search; Bounded context-switching;
Partial order reduction; Bitstate hashing; Software verification
AB We discuss the implementation of a bounded context switching algorithm in the Spin model checker. The algorithm allows us to find counter-examples that are often simpler to understand, and that may be more likely to occur in practice. We discuss extensions of the algorithm that allow us to use this new algorithm in combination with most other search modes supported in Spin, including partial order reduction and bitstate hashing. We show that, other than often assumed, the enforcement of a bounded context switching discipline does not decrease but increases the complexity of the model checking procedure. We discuss the performance of the algorithm on a range of applications.
C1 [Holzmann, Gerard J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Florian, Mihai] CALTECH, Dept Comp Sci, Pasadena, CA 91109 USA.
RP Holzmann, GJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-230, Pasadena, CA 91109 USA.
EM gerard@spinroot.com
NR 14
TC 7
Z9 8
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0934-5043
EI 1433-299X
J9 FORM ASP COMPUT
JI Form. Asp. Comput.
PD MAY
PY 2011
VL 23
IS 3
BP 365
EP 389
DI 10.1007/s00165-010-0160-5
PG 25
WC Computer Science, Software Engineering
SC Computer Science
GA 750DI
UT WOS:000289524500007
ER
PT J
AU Kay, RB
Poulios, D
Coyle, DB
Stysley, PR
Clarke, GB
AF Kay, Richard B.
Poulios, Demetrios
Coyle, Donald Barry
Stysley, Paul R.
Clarke, Gregory B.
TI Derivation of the Frantz-Nodvik Equation for Diode-Side-Pumped Zigzag
Slab Laser Amplifiers with Gaussian Laser Mode and Pump Beam Shapes
SO IEEE JOURNAL OF QUANTUM ELECTRONICS
LA English
DT Article
DE Laser diode-side-pumping; spatial pump distribution; zigzag slab
amplifiers
ID Q-SWITCHED LASER
AB The theory for Gaussian beam pulse propagation in a zigzag slab amplifier with a Gaussian pump distribution is detailed. Provisions are made for amplification of an input signal with an elliptical Gaussian spatial mode by modifying the time-dependent photon transport equations as described by Eggleston Frantz, and Injeyan. A comparison is made with experimental results of a diode-side-pumped zigzag slab amplifier element amplifying a near-Gaussian beam.
C1 [Kay, Richard B.; Poulios, Demetrios; Clarke, Gregory B.] American Univ, Dept Phys, Washington, DC 20016 USA.
[Coyle, Donald Barry; Stysley, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kay, RB (reprint author), American Univ, Dept Phys, Washington, DC 20016 USA.
EM Richard.B.Kay@nasa.gov; poulios@american.edu; Barry.Coyle@nasa.gov;
Paul.Stysley@nasa.gov; gc8795a@student.american.edu
FU National Aeronautics and Space Administration [NNX08AJ95A]; Laser
Physics Group, Department of Physics, American University, Washington
D.C., USA
FX This work was supported in part by the National Aeronautics and Space
Administration Cooperative Research under Agreement NNX08AJ95A with the
Laser Physics Group, Department of Physics, American University,
Washington D.C., USA.
NR 7
TC 1
Z9 1
U1 1
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9197
EI 1558-1713
J9 IEEE J QUANTUM ELECT
JI IEEE J. Quantum Electron.
PD MAY
PY 2011
VL 47
IS 5
BP 745
EP 749
DI 10.1109/JQE.2011.2114329
PG 5
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 749PF
UT WOS:000289480100007
ER
PT J
AU Schuet, S
Timucin, D
Wheeler, K
AF Schuet, Stefan
Timucin, Dogan
Wheeler, Kevin
TI A Model-Based Probabilistic Inversion Framework for Characterizing Wire
Fault Detection Using TDR
SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT
LA English
DT Article; Proceedings Paper
CT IEEE International Instrumentation and Measurement Conference
CY MAY 03-06, 2010
CL Austin, TX
SP IEEE
DE Bayesian; fault detection; S-parameters; time-domain reflectometry
(TDR); wiring
ID DOMAIN REFLECTOMETRY; WIRING FAULTS; LOCATION
AB Time-domain reflectometry (TDR) is one of the standard methods for diagnosing faults in electrical wiring and interconnect systems, with a long-standing history focused mainly on hardware development of both high-fidelity systems for laboratory use and portable handheld devices for field deployment. While these devices can easily assess distance to hard faults such as sustained opens or shorts, their ability to assess subtle but important degradation such as chafing remains an open question. This paper presents a unified framework for TDR-based chafing fault detection in lossy coaxial cables by combining an S-parameter-based forward-modeling approach with a probabilistic (Bayesian) inference algorithm. Results are presented for the estimation of nominal and faulty cable parameters from laboratory data.
C1 [Schuet, Stefan; Timucin, Dogan; Wheeler, Kevin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Schuet, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM stefan.r.schuet@nasa.gov; kevin.r.wheeler@nasa.gov
NR 17
TC 19
Z9 19
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9456
EI 1557-9662
J9 IEEE T INSTRUM MEAS
JI IEEE Trans. Instrum. Meas.
PD MAY
PY 2011
VL 60
IS 5
BP 1654
EP 1663
DI 10.1109/TIM.2011.2105030
PG 10
WC Engineering, Electrical & Electronic; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 745XH
UT WOS:000289204400017
ER
PT J
AU Bhatia, AK
Landi, E
AF Bhatia, A. K.
Landi, E.
TI Atomic data and spectral line intensities for Ni XVII
SO ATOMIC DATA AND NUCLEAR DATA TABLES
LA English
DT Article
ID EXTREME-ULTRAVIOLET SPECTRUM; ELECTRON-IMPACT EXCITATION; MG-LIKE IONS;
INTERCOMBINATION LINES; RATE COEFFICIENTS; EMISSION-LINES;
ENERGY-LEVELS; CA-IX; ISOELECTRONIC SEQUENCE; MAGNESIUM SEQUENCE
AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Ni XVII. We include in the calculations the 23 lowest configurations, corresponding to 159 fine-structure levels: 3l3l', 3l4l '', and 3s51", with l,l' = s,p,d, l '' = s,p,d, f, and l''' = s,p,d. Collision strengths are calculated at five incident energies for all transitions at varying energies above the threshold of each transition. One additional energy, very close to the threshold of each transition, has also been included. Calculations have been carried out using the Flexible Atomic Code in the distorted wave approximation. Additional calculations have been performed with the University College London suite of codes for comparison. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates of the present work, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(8) - 10(14) cm(-3) and at an electron temperature of log T(e)(K) = 6.5, corresponding to the maximum abundance of Ni XVII. Spectral line intensities are calculated, and their diagnostic relevance is discussed. This dataset will be made available in the next version of the CHIANTI database. (C) 2010 Published by Elsevier Inc.
C1 [Landi, E.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Landi, E.] USN, Res Lab, Washington, DC 20375 USA.
RP Landi, E (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA.
EM elandi@umich.edu
RI Landi, Enrico/H-4493-2011
FU NASA; [NNH06CD24C]; [NNG04ED07P]
FX The work of Enrico Landi is supported by the NNH06CD24C, NNG04ED07P, and
other NASA Grants. Calculations were carried out using the Discover
computer of the NASA Center for Computation Science.
NR 44
TC 5
Z9 6
U1 0
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0092-640X
J9 ATOM DATA NUCL DATA
JI Atom. Data Nucl. Data Tables
PD MAY
PY 2011
VL 97
IS 3
BP 189
EP 224
DI 10.1016/j.adt.2010.07.001
PG 36
WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear
SC Physics
GA 747OJ
UT WOS:000289329000001
ER
PT J
AU Norvig, P
Aldhous, P
AF Norvig, Peter
Aldhous, Peter
TI Google's data junkie
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [Norvig, Peter] NASA, Ames Res Ctr, Computat Sci Div, Washington, DC 20546 USA.
RP Norvig, P (reprint author), NASA, Ames Res Ctr, Computat Sci Div, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 1
U2 6
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 APR 30
PY 2011
VL 210
IS 2810
BP 26
EP 27
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 760AX
UT WOS:000290294300028
ER
PT J
AU Huang, JF
Hsu, NC
Tsay, SC
Jeong, MJ
Holben, BN
Berkoff, TA
Welton, EJ
AF Huang, Jingfeng
Hsu, N. Christina
Tsay, Si-Chee
Jeong, Myeong-Jae
Holben, Brent N.
Berkoff, Timothy A.
Welton, Ellsworth J.
TI Susceptibility of aerosol optical thickness retrievals to thin cirrus
contamination during the BASE-ASIA campaign
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RESOLUTION IMAGING SPECTRORADIOMETER; ACE-ASIA; CLOUD; SATELLITE;
AERONET; MODIS; ALGORITHMS; 1.38-MU-M; CHANNELS; IMPACTS
AB We used a combination of ground measurements (Aerosol Robotic Network, AERONET; Micro-Pulse Lidar Network, MPLNET) and satellite data (Moderate Resolution Imaging Spectroradiometer, MODIS; Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation, CALIPSO) to examine the susceptibility of ground and satellite aerosol retrievals to thin cirrus contamination at Phimai, Thailand (102.56 degrees E, 15.18 degrees N, also known as Pimai), during the Biomass-burning Aerosols in South East-Asia: Smoke Impact Assessment (BASE-ASIA) campaign (February-May 2006). Using the strengths of spaceborne or ground lidars to detect cirrus clouds, we conducted statistical analyses for four different scenarios: MPLNET versus AERONET, MPLNET versus MODIS, CALIPSO versus AERONET, and CALIPSO versus MODIS. Cirrus identifications from MPLNET or CALIPSO were paired up with concurrent aerosol optical thickness (AOT) measurements from AERONET or MODIS. Results from the BASE-ASIA campaign suggest that current operational AERONET and MODIS AOT products are influenced by thin cirrus contamination featuring strong seasonality. Concurrent AERONET and MPLNET observations indicate that additional thin cirrus screening changes AOT monthly means by 5%, with 20% of the AERONET aerosol data at Phimai being cirrus contaminated in boreal spring. From noncirrus cases to cirrus-contaminated cases, AERONET AOT increases along with larger particle sizes. We further evaluated the performance of eight MODIS-derived cirrus screening parameters for their effectiveness on thin cirrus screening: apparent reflectance at 1.38 mu m (R1.38), cirrus reflectance at 0.66 mu m (CR0.66), CR0.66 cirrus flag, reflectance ratio between 1.38 mu m and 0.66 mu m (RR1.38/0.66), reflectance ratio between 1.38 mu m and 1.24 mu m (RR1.38/1.24), brightness temperature difference between 8.6 mu m and 11 mu m (BTD8.6-11), brightness temperature difference between 11 mu m and 12 mu m (BTD11-12), and cloud phase infrared approach. Correlation analysis with the MPLNET cirrus flag indicates that RR1.38/0.66 is slightly preferable for high thin cirrus screening for the AERONET AOT measurements. The quantitative findings from this study suggest particular caution and careful evaluation of thin cirrus contamination in the satellite and ground AOT measurements before they are used for aerosol-related climatic forcing studies.
C1 [Huang, Jingfeng; Jeong, Myeong-Jae; Berkoff, Timothy A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Huang, Jingfeng; Hsu, N. Christina; Tsay, Si-Chee; Jeong, Myeong-Jae; Holben, Brent N.; Berkoff, Timothy A.; Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Huang, JF (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, 5523 Res Pk Dr, Baltimore, MD 21228 USA.
EM jfhuang@umbc.edu
RI Jeong, Myeong/B-8803-2008; Welton, Ellsworth/A-8362-2012; Huang,
Jingfeng/D-7336-2012; Hsu, N. Christina/H-3420-2013; Tsay,
Si-Chee/J-1147-2014
OI Huang, Jingfeng/0000-0002-8779-2922;
FU NASA EOS
FX This work is supported by a grant from the NASA EOS Program, managed by
Hal Maring. The authors thank Alexander Smirnov, David Giles, Bo-Cai
Gao, Richard A. Hansell, Steve Ou, and Zhien Wang for their constructive
comments on the use of in situ and satellite data, analysis methodology,
and cirrus climatology. The authors thank three anonymous reviewers for
their comments that were valuable to improving the paper. Aqua MODIS L1B
and L2 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.
NR 36
TC 36
Z9 36
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 30
PY 2011
VL 116
AR D08214
DI 10.1029/2010JD014910
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 757QT
UT WOS:000290103500002
ER
PT J
AU Seker, I
Fung, SF
Mathews, JD
AF Seker, Ilgin
Fung, Shing F.
Mathews, John D.
TI Relation between magnetospheric state parameters and the occurrence of
plasma depletion events in the nighttime midlatitude F region
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID TRAVELING IONOSPHERIC DISTURBANCES; EQUATORIAL SPREAD-F;
GEOMAGNETIC-ACTIVITY; RADAR; AIRGLOW; BUBBLES; INSTABILITY; ARECIBO;
NETWORK
AB Studies using all-sky imagers have revealed the presence of various ionospheric irregularities in the nighttime midlatitude F region. The most prevalent and well known of these are the medium-scale traveling ionospheric disturbances (MSTIDs) that usually occur when the geomagnetic activity is low and midlatitude spread F plumes that are often observed when the geomagnetic activity is high. The inverse and direct relations between geomagnetic activity and the occurrence rate of MSTIDs and midlatitude plumes, respectively, have been observed by several studies using different instruments; however, most of them focus on MSTIDs only and use only Kp to characterize geomagnetic activity. In order to understand the underlying causes of these two relations and to distinguish between MSTIDs and plumes, it is illuminating to better characterize the occurrence of MSTIDs and plumes using multiple magnetospheric state parameters. Here we statistically compare multiple geomagnetic driver and response parameters (such as Kp, AE, Dst, and solar wind parameters) with the occurrence rates of nighttime MSTIDs and plumes observed using an all-sky imager at Arecibo Observatory (AO) between 2003 and 2008. We also present seasonal and annual variations of MSTIDs and plumes at AO. The results not only allow us to better distinguish MSTIDs and plumes, but also to shed further light on the generation mechanism and electrodynamics of these two different phenomena occurring at nighttime in the midlatitude F region.
C1 [Seker, Ilgin; Fung, Shing F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Mathews, John D.] Penn State Univ, Radar Space Sci Lab, Dept Elect Engn, University Pk, PA 16902 USA.
RP Seker, I (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Code 632, Greenbelt, MD 20771 USA.
EM ilgin.seker@nasa.gov
RI Fung, Shing/F-5647-2012
FU NASA; NSF [ATM 07-21613]
FX 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 Penn State
All-Sky Imager System is supported under NSF grant ATM 07-21613 to
Pennsylvania State University. The monthly and annual variation plots
have been provided by NASA summer intern Seok Youl Yoon. We thank the
reviewers for their constructive comments.
NR 32
TC 4
Z9 4
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR 30
PY 2011
VL 116
AR A04323
DI 10.1029/2010JA015521
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 757RH
UT WOS:000290104900001
ER
PT J
AU Davami, K
Kang, D
Lee, JS
Meyyappan, M
AF Davami, Keivan
Kang, Daegun
Lee, Jeong-Soo
Meyyappan, M.
TI Synthesis of ZnTe nanostructures by vapor-liquid-solid technique (vol
504, pg 62, 2011)
SO CHEMICAL PHYSICS LETTERS
LA English
DT Correction
C1 [Davami, Keivan; Kang, Daegun; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang, South Korea.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lee, JS (reprint author), Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang, South Korea.
EM ljs6951@postech.ac.kr; m.meyyappan@nasa.gov
NR 1
TC 2
Z9 3
U1 1
U2 10
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 APR 29
PY 2011
VL 507
IS 1-3
BP 208
EP 208
DI 10.1016/j.cplett.2011.03.029
PG 1
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 753KP
UT WOS:000289772600040
ER
PT J
AU Sola, F
Hurwitz, F
Yang, J
AF Sola, F.
Hurwitz, F.
Yang, J.
TI A new scanning electron microscopy approach to image aerogels at the
nanoscale
SO NANOTECHNOLOGY
LA English
DT Article
ID IONIZATION CROSS-SECTIONS; LOW-VACUUM; EMISSION; SILICA; SEM
AB A new scanning electron microscopy (SEM) technique to image poor electrically conductive aerogels is presented. The process can be performed by non-expert SEM users. We showed that negative charging effects on aerogels can be minimized significantly by inserting dry nitrogen gas close to the region of interest. The process involves the local recombination of accumulated negative charges with positive ions generated from ionization processes. This new technique made possible the acquisition of images of aerogels with pores down to approximately 3 nm in diameter using a positively biased Everhart-Thornley (ET) detector.
C1 [Sola, F.; Hurwitz, F.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
[Yang, J.] Carl Zeiss NTS LLC, Peabody, MA 01960 USA.
RP Sola, F (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
EM francisco.sola-lopez@nasa.gov
FU Hypersonic Project in the Fundamental Aeronautics Program
FX This work was supported by the Hypersonic Project in the Fundamental
Aeronautics Program.
NR 24
TC 1
Z9 1
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD APR 29
PY 2011
VL 22
IS 17
AR 175704
DI 10.1088/0957-4484/22/17/175704
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 736QR
UT WOS:000288509700017
PM 21411927
ER
PT J
AU Li, XL
Palo, S
Kohnert, R
AF Li, Xinlin
Palo, Scott
Kohnert, Rick
TI Small Space Weather Research Mission Designed Fully by Students
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Editorial Material
C1 [Li, Xinlin; Kohnert, Rick] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Li, Xinlin; Palo, Scott] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Li, Xinlin] NASA, RBSP Mission, Washington, DC USA.
RP Li, XL (reprint author), Univ Colorado, LASP, Boulder, CO 80309 USA.
EM lix@lasp.colorado.edu
OI PALO, SCOTT/0000-0002-4729-4929
NR 0
TC 4
Z9 4
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR 28
PY 2011
VL 9
AR S04006
DI 10.1029/2011SW000668
PG 2
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 757QY
UT WOS:000290104000002
ER
PT J
AU Rastatter, L
Kuznetsova, MM
Vapirev, A
Ridley, A
Wiltberger, M
Pulkkinen, A
Hesse, M
Singer, HJ
AF Rastaetter, L.
Kuznetsova, M. M.
Vapirev, A.
Ridley, A.
Wiltberger, M.
Pulkkinen, A.
Hesse, M.
Singer, H. J.
TI Geospace Environment Modeling 2008-2009 Challenge: Geosynchronous
magnetic field
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID INNER MAGNETOSPHERE; SIMULATION; MAGNETOPAUSE; SUBSTORM; SCHEME; WIND
AB In this paper the metrics-based results of the inner magnetospheric magnetic field part of the 2008-2009 GEM Metrics Challenge are reported. The Metrics Challenge asked modelers to submit results for four geomagnetic storm events and five different types of observations that can be modeled by statistical or climatological or physics-based (e. g., MHD) models of the magnetosphere-ionosphere system. We present the results of 12 model settings that were run at the Community Coordinated Modeling Center and at the institutions of various modelers for these events. To measure the performance of each of the models against the observations, we use direct comparisons between the strength of the measured magnetic field (B), the sine of the elevation angle Theta(xz) (tau), and the spectral power of fluctuations for both quantities. We find that model rankings vary widely by type of variable and skill score used. None of the models consistently performs best for all events. We find that empirical models perform well for weak storm events, and physics-based (magnetohydrodynamic) models are better for strong storm events. Within a series of runs of the same model we find that higher resolution may not always improve results unless more physics of the inner magnetosphere, such as the kinetic description of the ring current, is included.
C1 [Rastaetter, L.; Kuznetsova, M. M.; Pulkkinen, A.; Hesse, M.] NASA, Community Coordinated Modeling Ctr, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Ridley, A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Singer, H. J.] NOAA, Space Weather Predict Ctr, Natl Ctr Environm Predict, Natl Weather Serv, Boulder, CO 80305 USA.
[Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Vapirev, A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Pulkkinen, A.] Catholic Univ Amer, IACS, Washington, DC 20064 USA.
RP Rastatter, L (reprint author), NASA, Community Coordinated Modeling Ctr, Space Weather Lab, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20770 USA.
EM lutz.rastaetter@nasa.gov; maria.m.kuznetsova@nasa.gov;
alexander.vapirev@unh.edu; ridley@umich.edu; wiltbemj@ucar.edu;
antti.a.pulkkinen@nasa.gov; michael.hesse@nasa.gov;
howard.singer@noaa.gov
RI Ridley, Aaron/F-3943-2011; Hesse, Michael/D-2031-2012; Rastaetter,
Lutz/D-4715-2012; Wiltberger, Michael/B-8781-2008
OI Ridley, Aaron/0000-0001-6933-8534; Rastaetter, Lutz/0000-0002-7343-4147;
Wiltberger, Michael/0000-0002-4844-3148
NR 24
TC 17
Z9 17
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR 28
PY 2011
VL 9
AR S04005
DI 10.1029/2010SW000617
PG 15
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 757QY
UT WOS:000290104000001
ER
PT J
AU Kersten, K
Cattell, CA
Breneman, A
Goetz, K
Kellogg, PJ
Wygant, JR
Wilson, LB
Blake, JB
Looper, MD
Roth, I
AF Kersten, K.
Cattell, C. A.
Breneman, A.
Goetz, K.
Kellogg, P. J.
Wygant, J. R.
Wilson, L. B., III
Blake, J. B.
Looper, M. D.
Roth, I.
TI Observation of relativistic electron microbursts in conjunction with
intense radiation belt whistler-mode waves
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MAGNETOSPHERIC CHORUS; VLF CHORUS; ASSOCIATION; MISSION; RADIO; SOLAR
AB We present multi-satellite observations of large amplitude radiation belt whistler-mode waves and relativistic electron precipitation. On separate occasions during the Wind petal orbits and STEREO phasing orbits, Wind and STEREO recorded intense whistler-mode waves in the outer nightside equatorial radiation belt with peak-to-peak amplitudes exceeding 300 mV/m. During these intervals of intense wave activity, SAMPEX recorded relativistic electron microbursts in near magnetic conjunction with Wind and STEREO. This evidence of microburst precipitation occurring at the same time and at nearly the same magnetic local time and L-shell with a bursty temporal structure similar to that of the observed large amplitude wave packets suggests a causal connection between the two phenomena. Simulation studies corroborate this idea, showing that nonlinear wave-particle interactions may result in rapid energization and scattering on timescales comparable to those of the impulsive relativistic electron precipitation. Citation: Kersten, K., C. A. Cattell, A. Breneman, K. Goetz, P. J. Kellogg, J. R. Wygant, L. B. Wilson III, J. B. Blake, M. D. Looper, and I. Roth (2011), Observation of relativistic electron microbursts in conjunction with intense radiation belt whistler-mode waves, Geophys. Res. Lett., 38, L08107, doi:10.1029/2011GL046810.
C1 [Kersten, K.; Cattell, C. A.; Breneman, A.; Goetz, K.; Kellogg, P. J.; Wygant, J. R.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Blake, J. B.; Looper, M. D.] Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA.
[Roth, I.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Wilson, L. B., III] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kersten, K (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
EM kkersten@physics.umn.edu
RI Wilson III, Lynn/D-4425-2012;
OI Wilson III, Lynn/0000-0002-4313-1970; Cattell,
Cynthia/0000-0002-3805-320X
FU NASA STEREO [NNX09AG82G, NNX07AF23G]; NASA, APL [NAS5-01072]
FX This work was supported by NASA STEREO grants NNX09AG82G and NNX07AF23G,
and by NASA grant NAS5-01072 under contract from APL for the development
of RBSP/EFW. Simulation work was carried out using resources of the
University of Minnesota Supercomputing Institute with the assistance of
Shuxia Zhang. Geosynchronous electron data provided by LANL. DST and AE
indices courtesy of WDC for Geomagnetism, Kyoto.
NR 24
TC 27
Z9 27
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2011
VL 38
AR L08107
DI 10.1029/2011GL046810
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 757SR
UT WOS:000290108500002
ER
PT J
AU Schinder, PJ
Flasar, FM
Marouf, EA
French, RG
McGhee, CA
Kliore, AJ
Rappaport, NJ
Barbinis, E
Fleischman, D
Anabtawi, A
AF Schinder, P. J.
Flasar, F. M.
Marouf, E. A.
French, R. G.
McGhee, C. A.
Kliore, A. J.
Rappaport, N. J.
Barbinis, E.
Fleischman, D.
Anabtawi, A.
TI Saturn's equatorial oscillation: Evidence of descending thermal
structure from Cassini radio occultations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID STRATOSPHERIC TEMPERATURES; MIDDLE ATMOSPHERE; ZONAL WINDS; JUPITER
AB A series of near-equatorial radio occultations of Cassini by Saturn occurred in 2005 and again in 2009-2010. Comparison of the temperature-pressure profiles obtained from the two sets of occultations shows evidence of a descending pattern in the stratosphere that is similar to those associated with equatorial oscillations in Earth's middle atmosphere. This is the first time that this descent has been observed in another planetary atmosphere. If absorption of upwardly propagating waves drives the descent, the implied absorbed flux is 0.05 m(2) s(-2), at least as large if not greater than on Earth. Citation: Schinder, P. J., F. M. Flasar, E. A. Marouf, R. G. French, C. A. McGhee, A. J. Kliore, N. J. Rappaport, E. Barbinis, D. Fleischman, and A. Anabtawi (2011), Saturn's equatorial oscillation: Evidence of descending thermal structure from Cassini radio occultations, Geophys. Res. Lett., 38, L08205, doi:10.1029/2011GL047191.
C1 [Schinder, P. J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Kliore, A. J.; Rappaport, N. J.; Barbinis, E.; Fleischman, D.; Anabtawi, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[French, R. G.; McGhee, C. A.] Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA.
[Marouf, E. A.] San Jose State Univ, Dept Elect Engn, San Jose, CA 95192 USA.
RP Schinder, PJ (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
EM schinder@astro.cornell.edu
RI Flasar, F Michael/C-8509-2012;
OI Schinder, Paul/0000-0002-4571-7895
NR 17
TC 8
Z9 8
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2011
VL 38
AR L08205
DI 10.1029/2011GL047191
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 757SR
UT WOS:000290108500007
ER
PT J
AU Nguyen, AT
Menemenlis, D
Kwok, R
AF Nguyen, An T.
Menemenlis, Dimitris
Kwok, Ronald
TI Arctic ice-ocean simulation with optimized model parameters: Approach
and assessment
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SEA-ICE; FRAM STRAIT; CIRCULATION; REANALYSIS; REPRESENTATION;
ASSIMILATION; VARIABILITY; TOPOGRAPHY; THICKNESS; DYNAMICS
AB We present an optimized 1992-2008 coupled ice-ocean simulation of the Arctic Ocean. A Green's function approach adjusts a set of parameters for best model-data agreement. Overall, model-data differences are reduced by 45%. The optimized simulation reproduces the negative trends in ice extent in the satellite records. Volume and thickness distributions are comparable to those from the Ice, Cloud, and land Elevation Satellite (2003-2008). The upper cold halocline is consistent with observations in the western Arctic. The freshwater budget of the Arctic Ocean and volume/heat transports of Pacific and Atlantic waters across major passages are comparable with observation-based estimates. We note that the optimized parameters depend on the selected atmospheric forcing. The use of the 25 year Japanese reanalysis results in sea ice albedos that are consistent with field observations. Simulated Pacific Water enters the Bering Strait and flows off the Chukchi Shelf along four distinct channels. This water takes similar to 5-10 years to exit the Arctic Ocean at the Canadian Arctic Archipelago, Nares, or Fram straits. Atlantic Water entering the Fram Strait flows eastward, merges with the St Ana Trough inflow, and splits into two branches at the southwest corner of the Makarov Basin. One branch flows along Lomonosov Ridge back to Fram Strait. The other enters the western Arctic, circulates cyclonically below the halocline, and exits mainly through the Nares and Fram straits. This work utilizes the record of available observations to obtain an Arctic Ocean simulation that is in agreement with observations both within and beyond the optimization period and that can be used for tracer and process studies.
C1 [Nguyen, An T.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Nguyen, An T.; Menemenlis, Dimitris; Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nguyen, AT (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM an.t.nguyen@jpl.nasa.gov; dimitris.menemenlis@jpl.nasa.gov;
ronald.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU ECCO2 project; NASA Advanced Supercomputing (NAS) Division; JPL
Supercomputing and Visualization Facility (SVF)
FX Sea ice draft data were downloaded from the National Snow and Ice Data
Center (NSIDC). This work is funded by 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 and from the JPL Supercomputing
and Visualization Facility (SVF).
NR 82
TC 48
Z9 51
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR 27
PY 2011
VL 116
AR C04025
DI 10.1029/2010JC006573
PG 18
WC Oceanography
SC Oceanography
GA 757SK
UT WOS:000290107800002
ER
PT J
AU Hand, KP
Khurana, KK
Chyba, CF
AF Hand, K. P.
Khurana, K. K.
Chyba, C. F.
TI Joule heating of the south polar terrain on Enceladus
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID VAPOR PLUMES; PLASMA TORUS; IO; EUROPA; SODIUM; OCEAN; WATER
AB We report that Joule heating in Enceladus, resulting from the interaction of Enceladus with Saturn's magnetic field, may account for 150 kW to 52 MW of power through Enceladus. Electric currents passing through subsurface channels of low salinity and just a few kilometers in depth could supply a source of power to the south polar terrain, providing a small but previously unaccounted for contribution to the observed heat flux and plume activity. Studies of the electrical heating of Jupiter's moon Europa have concluded that electricity is a negligible heating source since no connection between the conductive subsurface and Alfven currents has been observed. Here we show that, contrary to results for the Jupiter system, electrical heating may be a source of internal energy for Enceladus, contributing to localized heating, production of water vapor, and the persistence of the "tiger stripes." This contribution is of order 0.001-0.25% of the total observed heat flux, and thus, Joule heating cannot explain the total south polar terrain heat anomaly. The exclusion of salt ions during refreezing serves to enhance volumetric Joule heating and could extend the lifetime of liquid water fractures in the south polar terrain.
C1 [Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chyba, C. F.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Khurana, K. K.] Univ Calif Los Angeles, Dept Planetary Sci, Los Angeles, CA 90095 USA.
RP Hand, KP (reprint author), CALTECH, Jet Prop Lab, MS 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Kevin.P.Hand@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology; NASA;
NASA Astrobiology Institute, Astrobiology of Icy Worlds' team at the Jet
Propulsion Laboratory
FX K. P. Hand acknowledges support from the Jet Propulsion Laboratory,
California Institute of Technology, through a contract with NASA, and
support through the NASA Astrobiology Institute, Astrobiology of Icy
Worlds' team at the Jet Propulsion Laboratory.
NR 35
TC 2
Z9 2
U1 0
U2 2
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 APR 27
PY 2011
VL 116
AR E04010
DI 10.1029/2010JE003776
PG 5
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 757TD
UT WOS:000290109700001
ER
PT J
AU Isaacson, PJ
Pieters, CM
Besse, S
Clark, RN
Head, JW
Klima, RL
Mustard, JF
Petro, NE
Staid, MI
Sunshine, JM
Taylor, LA
Thaisen, KG
Tompkins, S
AF Isaacson, Peter J.
Pieters, Carle M.
Besse, Sebastien
Clark, Roger N.
Head, James W.
Klima, Rachel L.
Mustard, John F.
Petro, Noah E.
Staid, Matthew I.
Sunshine, Jessica M.
Taylor, Lawrence A.
Thaisen, Kevin G.
Tompkins, Stefanie
TI Remote compositional analysis of lunar olivine-rich lithologies with
Moon Mineralogy Mapper (M-3) spectra
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID CLEMENTINE NIR DATA; REFLECTANCE SPECTROSCOPY; OPTICAL-PROPERTIES;
CRATER COPERNICUS; MARE BASALTS; SPACE; IRON; SIMULATION; ARISTARCHUS;
ASTEROIDS
AB A systematic approach for deconvolving remotely sensed lunar olivine-rich visible to near-infrared (VNIR) reflectance spectra with the Modified Gaussian Model (MGM) is evaluated with Chandrayaan-1 Moon Mineralogy Mapper (M-3) spectra. Whereas earlier studies of laboratory reflectance spectra focused only on complications due to chromite inclusions in lunar olivines, we develop a systematic approach for addressing (through continuum removal) the prominent continuum slopes common to remotely sensed reflectance spectra of planetary surfaces. We have validated our continuum removal on a suite of laboratory reflectance spectra. Suites of olivine-dominated reflectance spectra from a small crater near Mare Moscoviense, the Copernicus central peak, Aristarchus, and the crater Marius in the Marius Hills were analyzed. Spectral diversity was detected in visual evaluation of the spectra and was quantified using the MGM. The MGM-derived band positions are used to estimate the olivine's composition in a relative sense. Spectra of olivines from Moscoviense exhibit diversity in their absorption features, and this diversity suggests some variation in olivine Fe/Mg content. Olivines from Copernicus are observed to be spectrally homogeneous and thus are predicted to be more compositionally homogeneous than those at Moscoviense but are of broadly similar composition to the Moscoviense olivines. Olivines from Aristarchus and Marius exhibit clear spectral differences from those at Moscoviense and Copernicus but also exhibit features that suggest contributions from other phases. If the various precautions discussed here are weighed carefully, the methods presented here can be used to make general predictions of absolute olivine composition (Fe/Mg content).
C1 [Isaacson, Peter J.; Pieters, Carle M.; Head, James W.; Mustard, John F.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Besse, Sebastien; Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
[Klima, Rachel L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA.
[Petro, Noah E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Staid, Matthew I.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Taylor, Lawrence A.; Thaisen, Kevin G.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[Tompkins, Stefanie] Def Adv Res Projects Agcy, Arlington, VA 22203 USA.
RP Isaacson, PJ (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA.
EM Peter_Isaacson@Brown.edu
RI Klima, Rachel/H-9383-2012; Petro, Noah/F-5340-2013;
OI Klima, Rachel/0000-0002-9151-6429; Besse, Sebastien/0000-0002-1052-5439
FU NASA [NNM05AB26C]; NASA LSI at Brown University [NNA09DB34A]
FX The efforts of the entire M3 engineering, operations, and
science teams are gratefully acknowledged. M3 science
validation is supported through NASA contract NNM05AB26C. M3
is supported as a NASA Discovery Program mission of opportunity. The
M3 team is grateful to ISRO for the opportunity to fly as a
guest instrument on Chandrayaan-1. Partial funding for this analysis has
also been provided through the NASA LSI at Brown University under
contract NNA09DB34A. Careful reviews by Brett Denevi and an anonymous
reviewer have improved this manuscript substantially. The views,
opinions, and/or findings contained in this paper are those of the
authors and should not be interpreted as representing the official
views, either expressed or implied, of the Defense Advanced Research
Projects Agency or the Department of Defense.
NR 59
TC 32
Z9 37
U1 0
U2 13
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 APR 26
PY 2011
VL 116
AR E00G11
DI 10.1029/2010JE003731
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 757TA
UT WOS:000290109400002
ER
PT J
AU Phebus, BD
Johnson, AV
Mar, B
Stone, BM
Colaprete, A
Iraci, LT
AF Phebus, Bruce D.
Johnson, Alexandria V.
Mar, Brendan
Stone, Bradley M.
Colaprete, Anthony
Iraci, Laura T.
TI Water ice nucleation characteristics of JSC Mars-1 regolith simulant
under simulated Martian atmospheric conditions
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; MINERAL DUST PARTICLES; CLOUD FORMATION;
VAPOR; TEMPERATURES; PATHFINDER; SURROGATES; EVOLUTION; CHAMBER; CLIMATE
AB Water ice clouds in the Martian atmosphere are governed by parameters such as number density and particle size distribution that in turn affect how they influence the climate. With some of the underlying properties of cloud formation well known only for Earth, extrapolations to Mars are potentially misleading. We report here continued laboratory experiments to identify critical onset conditions for water ice formation under Martian cloud forming temperatures and water partial pressures (155-182 K, 7.6 x 10(-5) to 7.7 x 10(-3) Pa H(2)O). By observing the 3 mu m infrared band to monitor nucleation and growth, we observe significant temperature dependence in the nucleation of ice on JSC Mars-1 regolith simulant, with critical saturation ratios, S(crit), as high as 3.8 at 155 K. At temperatures below similar to 180 K, ice nucleation on JSC Mars-1 requires significant supersaturation, potentially impacting the Martian hydrological cycle.
C1 [Phebus, Bruce D.; Johnson, Alexandria V.; Mar, Brendan; Colaprete, Anthony; Iraci, Laura T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Phebus, Bruce D.; Mar, Brendan; Stone, Bradley M.] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA.
[Johnson, Alexandria V.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA.
RP Phebus, BD (reprint author), Univ Calif Santa Cruz, Dept Chem & Biochem, 1156 High St, Santa Cruz, CA 95064 USA.
EM laura.t.iraci@nasa.gov
OI Phebus, Bruce/0000-0003-3489-5546
FU NASA
FX Thanks are due to D. Scimeca and E. Quigley for construction of the
apparatus. O. Marcu and M. Sanchez made possible the micrographs of the
JSC Mars-1 samples. Useful conversations with R. Terrill, A. Maattanen,
and M. Trainer are gratefully acknowledged. Funding for this work was
provided by the NASA Planetary Atmospheres Program (P. Crane, Program
Officer) with additional assistance provided from the NASA Undergraduate
Student Research Program (A.V.J).
NR 46
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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 APR 26
PY 2011
VL 116
AR E04009
DI 10.1029/2010JE003699
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 757TA
UT WOS:000290109400001
ER
PT J
AU Staid, MI
Pieters, CM
Besse, S
Boardman, J
Dhingra, D
Green, R
Head, JW
Isaacson, P
Klima, R
Kramer, G
Mustard, JM
Runyon, C
Sunshine, J
Taylor, LA
AF Staid, M. I.
Pieters, C. M.
Besse, S.
Boardman, J.
Dhingra, D.
Green, R.
Head, J. W.
Isaacson, P.
Klima, R.
Kramer, G.
Mustard, J. M.
Runyon, C.
Sunshine, J.
Taylor, L. A.
TI The mineralogy of late stage lunar volcanism as observed by the Moon
Mineralogy Mapper on Chandrayaan-1
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID INFRARED SPECTRAL REFLECTANCE; PROCELLARUM KREEP TERRANE; PROSPECTOR
GAMMA-RAY; MARE BASALTS; OCEANUS PROCELLARUM; CLEMENTINE MISSION; IRON;
OLIVINE; TIO2; SPECTROMETER
AB The last major phases of lunar volcanism produced spectrally unique high-titanium basalts on the western nearside of the Moon. The Moon Mineralogy Mapper (M-3) on Chandrayaan-1 has provided detailed measurements of these basalts at spatial and spectral resolutions necessary for mineralogical interpretation and mapping of distinct compositional units. The M-3 imaging spectrometer acquired data in 85 spectral bands from similar to 430 to 3000 nm at 140 to 280 m/pixel in its global mapping mode during the first half of 2009. Reflectance data of several key sites in the western maria were also acquired at higher spatial and spectral resolutions using M-3's target mode, prior to the end of the Chandrayaan-1 mission. These new observations confirm that both fresh craters and mare soils within the western high-Ti basalts display strong 1 mm and weak 2 mm absorptions consistent with olivine-rich basaltic compositions. The inferred abundance of olivine is observed to correlate with stratigraphic sequence across different mare regions and absolute ages. The apparent stratigraphic evolution and Fe-rich compositions of these basalts as a whole suggest an origin from evolved residual melts rather than through the assimilation of more primitive olivine-rich sources. Mare deposits with spectral properties similar to these late stage high-Ti basalts appear to be very limited outside the Procellarum-Imbrium region of the Moon and, where present, appear to occur as small areas of late stage regional volcanism. Detailed analyses of these new data and supporting measurements are in progress to provide further constraints on the mineralogy, olivine abundance, and compositions of these final products of lunar volcanism and the nature and evolution of their source regions.
C1 [Staid, M. I.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Pieters, C. M.; Dhingra, D.; Head, J. W.; Isaacson, P.; Mustard, J. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Besse, S.; Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Boardman, J.] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA.
[Green, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Klima, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA.
[Kramer, G.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Runyon, C.] Coll Charleston, Dept Geol, Charleston, SC 29424 USA.
[Taylor, L. A.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
RP Staid, MI (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Ste 106, Tucson, AZ 85719 USA.
EM staid@psi.edu
OI Besse, Sebastien/0000-0002-1052-5439
FU NASA [NNM05AB26C]
FX M3 is funded as a mission of opportunity through the NASA
Discovery program. The M3 science team and science validation
are supported through NASA contract NNM05AB26C. We thank ISRO for the
opportunity to fly as a guest instrument on Chandrayaan-1 and gratefully
acknowledge their many contributions to the acquisition and return of
the M3 data.
NR 102
TC 28
Z9 30
U1 3
U2 14
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 APR 26
PY 2011
VL 116
AR E00G10
DI 10.1029/2010JE003735
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 757TA
UT WOS:000290109400003
ER
PT J
AU Smith, DM
Dwyer, JR
Hazelton, BJ
Grefenstette, BW
Martinez-McKinney, GFM
Zhang, ZY
Lowell, AW
Kelley, NA
Splitt, ME
Lazarus, SM
Ulrich, W
Schaal, M
Saleh, ZH
Cramer, E
Rassoul, HK
Cummer, SA
Lu, G
Blakeslee, RJ
AF Smith, D. M.
Dwyer, J. R.
Hazelton, B. J.
Grefenstette, B. W.
Martinez-McKinney, G. F. M.
Zhang, Z. Y.
Lowell, A. W.
Kelley, N. A.
Splitt, M. E.
Lazarus, S. M.
Ulrich, W.
Schaal, M.
Saleh, Z. H.
Cramer, E.
Rassoul, H. K.
Cummer, S. A.
Lu, G.
Blakeslee, R. J.
TI The rarity of terrestrial gamma-ray flashes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID INTRACLOUD LIGHTNING DISCHARGES; RUNAWAY BREAKDOWN; ELECTRIC-FIELDS;
X-RAYS; THUNDERSTORMS; INITIATION; BURSTS; AIR
AB We report on the first search for Terrestrial Gamma-ray Flashes (TGFs) from altitudes where they are thought to be produced. The Airborne Detector for Energetic Lightning Emissions (ADELE), an array of gamma-ray detectors, was flown near the tops of Florida thunderstorms in August/September 2009. The plane passed within 10 km horizontal distance of 1213 lightning discharges and only once detected a TGF. If these discharges had produced TGFs of the same intensity as those seen from space, every one should have been seen by ADELE. Separate and significant nondetections are established for intracloud lightning, negative cloud-to-ground lightning, and narrow bipolar events. We conclude that TGFs are not a primary triggering mechanism for lightning. We estimate the TGF-to-flash ratio to be on the order of 10(-2) to 10(-3) and show that TGF intensities cannot follow the well-known power-law distribution seen in earthquakes and solar flares, due to our limits on the presence of faint events. Citation: Smith, D. M., et al. (2011), The rarity of terrestrial gamma-ray flashes, Geophys. Res. Lett., 38, L08807, doi: 10.1029/2011GL046875.
C1 [Smith, D. M.; Martinez-McKinney, G. F. M.; Zhang, Z. Y.; Kelley, N. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Smith, D. M.; Martinez-McKinney, G. F. M.; Zhang, Z. Y.; Kelley, N. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Smith, D. M.; Lowell, A. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Dwyer, J. R.; Schaal, M.; Saleh, Z. H.; Cramer, E.; Rassoul, H. K.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Hazelton, B. J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Grefenstette, B. W.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Splitt, M. E.; Lazarus, S. M.; Ulrich, W.] Florida Inst Technol, Dept Marine & Environm Syst, Melbourne, FL 32901 USA.
[Cummer, S. A.; Lu, G.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
[Blakeslee, R. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
RP Smith, DM (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, 1156 High St, Santa Cruz, CA 95064 USA.
EM dsmith@scipp.ucsc.edu
RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008;
OI Cummer, Steven/0000-0002-0002-0613; Rassoul, Hamid Kyan
Sam/0000-0003-0681-7276; Lazarus, Steven/0000-0002-5918-1059
FU NSF [ATM-0619941, ATM-0846609]
FX We thank Allen Schanot, the managing scientist of our field campaign
from NCAR/EOL; the other NCAR scientists who filled this role earlier or
helped us with GV data: Pavel Romashkin, Jorgen Jensen, and Jeff Stith;
and the EOL pilots, engineers, and technicians who provided exemplary
support. We also thank Stan Heckman of Weatherbug/AWS, not only for
providing sferic data, but for significant personal attention in helping
us interpret the data. ADELE was funded by NSF Major Research
Instrumentation grant ATM-0619941. Our simulation work was supported by
NSF grant ATM-0846609.
NR 30
TC 20
Z9 20
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 22
PY 2011
VL 38
AR L08807
DI 10.1029/2011GL046875
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 754LD
UT WOS:000289855200003
ER
PT J
AU Tosca, MG
Randerson, JT
Zender, CS
Nelson, DL
Diner, DJ
Logan, JA
AF Tosca, M. G.
Randerson, J. T.
Zender, C. S.
Nelson, D. L.
Diner, D. J.
Logan, J. A.
TI Dynamics of fire plumes and smoke clouds associated with peat and
deforestation fires in Indonesia
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID FOREST-FIRE; SATELLITE-OBSERVATIONS; MARITIME CONTINENT; EQUATORIAL
ASIA; EL-NINO; BIOMASS; EMISSIONS; TRANSPORT; CONVECTION; POLLUTION
AB During the dry season, anthropogenic fires in tropical forests and peatlands of equatorial Asia produce regionally expansive smoke clouds that have important effects on atmospheric radiation and air quality. Here we estimated the height of smoke on Borneo and Sumatra and characterized its sensitivity to El Nino and regional drought. We used Multiangle Imaging Spectroradiometer (MISR) satellite data and the MISR Interactive Explorer (MINX) software to estimate the heights of 317 smoke plumes on Borneo and 139 plumes on Sumatra during 2001-2009. In addition, we estimated the altitudes of larger smoke regions (smoke clouds) over Borneo using data from MISR and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) products. Most smoke plumes on Borneo (83%) were observed during El Nino years. Annually averaged plume heights on Borneo were significantly higher during El Nino events. Mean MISR-derived plume heights were 709 +/- 14 m on Borneo and 749 +/- 24 m on Sumatra during 2001-2009, with 96% of all plumes confined to within 500 m of the atmospheric boundary layer. Smoke clouds on Borneo were observed at altitudes between 1000 and 2000 m as measured by both MISR and CALIPSO. The difference in height between individual plumes and longer-lived regional smoke clouds may be related to deeper planetary boundary layers and higher-intensity fires later in the afternoon or other atmospheric mixing processes that occur on synoptic time scales. Our measurements and analyses suggested that direct injection of smoke into the free troposphere within fire plumes was not an important mechanism for vertical mixing of aerosols in equatorial Asia.
C1 [Tosca, M. G.; Randerson, J. T.; Zender, C. S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Nelson, D. L.; Diner, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Logan, J. A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
RP Tosca, MG (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM mtosca@uci.edu
RI Zender, Charles/D-4485-2012; Tosca, Michael/J-4908-2015
OI Zender, Charles/0000-0003-0129-8024; Tosca, Michael/0000-0003-1301-8341
FU NSF [ATM-0628637, ARC-0714088]; NASA [NNX08AF64G, 08-Earth08F-189,
NNX07AR23G]
FX The data presented here are publicly available in a database of plume
injection heights
(http://misr.jpl.nasa.gov/getData/accessData/MisrMinxPlumes/). We thank
three anonymous reviewers for critical analysis and insightful comments
about the interpretation of our results. We thank Ralph Kahn for advice
on comparisons between MISR and CALIPSO altitudes. We are grateful for
support from NSF (ATM-0628637) and NASA (NNX08AF64G). M. G. T. received
support from a NASA Earth and Space Science Fellowship
(08-Earth08F-189). C.S.Z. acknowledges NSF (ARC-0714088) and NASA
(NNX07AR23G) support. The MINX plume digitizing tool is publicly
available for Apple and PC users and can be downloaded at:
http://www.openchannelfoundation.org/projects/MINX.
NR 46
TC 44
Z9 44
U1 4
U2 38
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 APR 22
PY 2011
VL 116
AR D08207
DI 10.1029/2010JD015148
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 754KJ
UT WOS:000289853200004
ER
PT J
AU Kramer, GY
Combe, JP
Harnett, EM
Hawke, BR
Noble, SK
Blewett, DT
McCord, TB
Giguere, TA
AF Kramer, Georgiana Y.
Combe, Jean-Philippe
Harnett, Erika M.
Hawke, Bernard Ray
Noble, Sarah K.
Blewett, David T.
McCord, Thomas B.
Giguere, Thomas A.
TI Characterization of lunar swirls at Mare Ingenii: A model for space
weathering at magnetic anomalies
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID SOLAR-WIND; OPTICAL-PROPERTIES; FINEST FRACTION; ION IRRADIATION;
CLEMENTINE DATA; IMPACT CRATERS; MOON; SURFACE; MATURITY; MERCURY
AB Analysis of spectra from the Clementine ultraviolet-visible and near-infrared cameras of small, immature craters and surface soils both on and adjacent to the lunar swirls at Mare Ingenii has yielded the following conclusions about space weathering at a magnetic anomaly. (1) Despite having spectral characteristics of immaturity, the lunar swirls are not freshly exposed surfaces. (2) The swirl surfaces are regions of retarded weathering, while immediately adjacent regions experience accelerated weathering. (3) Weathering in the off-swirl regions darkens and flattens the spectrum with little to no reddening, which suggests that the production of larger (>40 nm) nanophase iron dominates in these locations as a result of charged particle sorting by the magnetic field. Preliminary analysis of two other lunar swirl regions, Reiner Gamma and Mare Marginis, is consistent with our observations at Mare Ingenii. Our results indicate that sputtering/vapor deposition, implanted solar wind hydrogen, and agglutination share responsibility for creating the range in npFe(0) particle sizes responsible for the spectral effects of space weathering.
C1 [Kramer, Georgiana Y.; Combe, Jean-Philippe; McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Harnett, Erika M.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Hawke, Bernard Ray; Giguere, Thomas A.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Noble, Sarah K.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Blewett, David T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Giguere, Thomas A.] Intergraph Corp, Kapolei, HI 96706 USA.
RP Kramer, GY (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM kramer@lpi.usra.edu
RI Noble, Sarah/D-7614-2012; Blewett, David/I-4904-2012
OI Blewett, David/0000-0002-9241-6358
NR 117
TC 18
Z9 18
U1 0
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 APR 22
PY 2011
VL 116
AR E04008
DI 10.1029/2010JE003669
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 754JX
UT WOS:000289852000001
ER
PT J
AU Pieters, CM
Besse, S
Boardman, J
Buratti, B
Cheek, L
Clark, RN
Combe, JP
Dhingra, D
Goswami, JN
Green, RO
Head, JW
Isaacson, P
Klima, R
Kramer, G
Lundeen, S
Malaret, E
McCord, T
Mustard, J
Nettles, J
Petro, N
Runyon, C
Staid, M
Sunshine, J
Taylor, LA
Thaisen, K
Tompkins, S
Whitten, J
AF Pieters, C. M.
Besse, S.
Boardman, J.
Buratti, B.
Cheek, L.
Clark, R. N.
Combe, J. P.
Dhingra, D.
Goswami, J. N.
Green, R. O.
Head, J. W.
Isaacson, P.
Klima, R.
Kramer, G.
Lundeen, S.
Malaret, E.
McCord, T.
Mustard, J.
Nettles, J.
Petro, N.
Runyon, C.
Staid, M.
Sunshine, J.
Taylor, L. A.
Thaisen, K.
Tompkins, S.
Whitten, J.
TI Mg-spinel lithology: A new rock type on the lunar farside
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID REFLECTANCE SPECTROSCOPY; SELENE; IMPACT; CAMERA; FIELD; MOON;
GEOTHERMOMETRY; PETROGENESIS; INSTRUMENT; PYROXENES
AB High-resolution compositional data from Moon Mineralogy Mapper (M-3) for the Moscoviense region on the lunar farside reveal three unusual, but distinctive, rock types along the inner basin ring. These are designated "OOS" since they are dominated by high concentrations of orthopyroxene, olivine, and Mg-rich spinel, respectively. The OOS occur as small areas, each a few kilometers in size, that are widely separated within the highly feldspathic setting of the basin rim. Although the abundance of plagioclase is not well constrained within the OOS, the mafic mineral content is exceptionally high, and two of the rock types could approach pyroxenite and harzburgite in composition. The third is a new rock type identified on the Moon that is dominated by Mg-rich spinel with no other mafic minerals detectable (<5% pyroxene, olivine). All OOS surfaces are old and undisturbed since basin formation. They are effectively invisible in image data and are only recognized by their distinctive composition identified spectroscopically. The origin of these unusual lithologies appears to be linked to one or more magmatic intrusions into the lower crust, perhaps near the crust-mantle interface. Processes such as fractional crystallization and gravity settling within such intrusions may provide a mechanism for concentrating the mafic components within zones several kilometers in dimension. The OOS are embedded within highly anorthositic material from the lunar crust; they may thus be near contemporaneous with crustal products from the cooling magma ocean.
C1 [Pieters, C. M.; Cheek, L.; Dhingra, D.; Head, J. W.; Isaacson, P.; Mustard, J.; Nettles, J.; Whitten, J.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Besse, S.; Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Boardman, J.] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA.
[Buratti, B.; Green, R. O.; Lundeen, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clark, R. N.] US Geol Survey, Fed Ctr, Denver, CO 80225 USA.
[Combe, J. P.; Kramer, G.; McCord, T.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Goswami, J. N.] NAVRANGPURA THALTEJ, ISRO, Phys Res Lab, Ahmadabad 380009, Gujarat, India.
[Klima, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA.
[Malaret, E.] Appl Coherent Technol Corp, Herndon, VA 22070 USA.
[Petro, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Runyon, C.] Coll Charleston, Dept Geol, Charleston, SC 29424 USA.
[Staid, M.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Taylor, L. A.; Thaisen, K.] Univ Tennessee, Planetary Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Tompkins, S.] Def Adv Res Projects Agcy, Arlington, VA 22203 USA.
RP Pieters, CM (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA.
EM carle_pieters@Brown.edu
RI Klima, Rachel/H-9383-2012; Petro, Noah/F-5340-2013;
OI Klima, Rachel/0000-0002-9151-6429; Besse, Sebastien/0000-0002-1052-5439
FU NASA [NNM05AB26C]
FX M3 is supported as a NASA Discovery Program mission of
opportunity. These science results and science validation is supported
through NASA contract NNM05AB26C. The M3 team is honored to
have had the opportunity to fly as a guest instrument on Chandrayaan-1,
and we are grateful to all the ISRO team that enabled M3 data
to be returned. We gratefully acknowledge the valuable input to this
project by the Chandrayaan-1 Terrain Mapping Camera team led by K. Kumar
and by the public release of SELENE Terrain Camera data and LRO Narrow
Angle Camera data. We appreciate the helpful review comments by Brad
Jolliff.
NR 51
TC 51
Z9 56
U1 1
U2 19
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 APR 22
PY 2011
VL 116
AR E00G08
DI 10.1029/2010JE003727
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 754JX
UT WOS:000289852000003
ER
PT J
AU Ruff, SW
Farmer, JD
Calvin, WM
Herkenhoff, KE
Johnson, JR
Morris, RV
Rice, MS
Arvidson, RE
Bell, JF
Christensen, PR
Squyres, SW
AF Ruff, Steven W.
Farmer, Jack D.
Calvin, Wendy M.
Herkenhoff, Kenneth E.
Johnson, Jeffrey R.
Morris, Richard V.
Rice, Melissa S.
Arvidson, Raymond E.
Bell, James F., III
Christensen, Philip R.
Squyres, Steven W.
TI Characteristics, distribution, origin, and significance of opaline
silica observed by the Spirit rover in Gusev crater, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID TAUPO VOLCANIC ZONE; THERMAL EMISSION-SPECTROSCOPY;
YELLOWSTONE-NATIONAL-PARK; NEW-ZEALAND; HYDROTHERMAL ALTERATION;
PARTICULATE SURFACES; REFLECTANCE SPECTRA; GEOTHERMAL FIELDS; SPRING
DEPOSITS; LOW-TEMPERATURE
AB The presence of outcrops and soil (regolith) rich in opaline silica (similar to 65-92 wt % SiO2) in association with volcanic materials adjacent to the "Home Plate" feature in Gusev crater is evidence for hydrothermal conditions. The Spirit rover has supplied a diverse set of observations that are used here to better understand the formation of silica and the activity, abundance, and fate of water in the first hydrothermal system to be explored in situ on Mars. We apply spectral, chemical, morphological, textural, and stratigraphic observations to assess whether the silica was produced by acid sulfate leaching of precursor rocks, by precipitation from silica-rich solutions, or by some combination. The apparent lack of S enrichment and the relatively low oxidation state of the Home Plate silica-rich materials appear inconsistent with the originally proposed Hawaiian analog for fumarolic acid sulfate leaching. The stratiform distribution of the silica-rich outcrops and their porous and brecciated microtextures are consistent with sinter produced by silica precipitation. There is no evidence for crystalline quartz phases among the silica occurrences, an indication of the lack of diagenetic maturation following the production of the amorphous opaline phase.
C1 [Ruff, Steven W.; Farmer, Jack D.; Christensen, Philip R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Calvin, Wendy M.] Univ Nevada, Dept Geol Sci, Reno, NV 89557 USA.
[Herkenhoff, Kenneth E.; Johnson, Jeffrey R.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA.
[Morris, Richard V.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Rice, Melissa S.; Bell, James F., III; Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Arvidson, Raymond E.] Washington Univ, Dept Planetary Sci, St Louis, MO 63130 USA.
RP Ruff, SW (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Moeur Bldg,Rm 131,Box 876305, Tempe, AZ 85287 USA.
EM steve.ruff@asu.edu
RI Johnson, Jeffrey/F-3972-2015
FU NASA
FX This work was funded in part by NASA grants from the Mars Data Analysis
and Mars Fundamental Research programs. We thank Patrick Browne and an
anonymous reviewer for their thorough and thoughtful reviews of a very
lengthy manuscript. Their suggestions have improved the final paper.
NR 88
TC 47
Z9 47
U1 3
U2 31
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 APR 22
PY 2011
VL 116
AR E00F23
DI 10.1029/2010JE003767
PG 48
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 754JX
UT WOS:000289852000005
ER
PT J
AU Laurent, P
Rodriguez, J
Wilms, J
Bel, MC
Pottschmidt, K
Grinberg, V
AF Laurent, P.
Rodriguez, J.
Wilms, J.
Bel, M. Cadolle
Pottschmidt, K.
Grinberg, V.
TI Polarized Gamma-Ray Emission from the Galactic Black Hole Cygnus X-1
SO SCIENCE
LA English
DT Article
ID BROAD-BAND SPECTRUM; X-RAY; ACCRETION DISKS; LOW/HARD STATE; RADIATION;
JETS; TELESCOPE; IBIS
AB Because of their inherently high flux allowing the detection of clear signals, black hole x-ray binaries are interesting candidates for polarization studies, even if no polarization signals have been observed from them before. Such measurements would provide further detailed insight into these sources' emission mechanisms. We measured the polarization of the gamma-ray emission from the black hole binary system Cygnus X-1 with the International Gamma-Ray Astrophysics Laboratory Imager on Board the Integral Satellite (INTEGRAL/IBIS) telescope. Spectral modeling of the data reveals two emission mechanisms: The 250- to 400-keV ( kilo-electron volt) data are consistent with emission dominated by Compton scattering on thermal electrons and are weakly polarized. The second spectral component seen in the 400-keV to 2-MeV band is by contrast strongly polarized, revealing that the MeV emission is probably related to the jet first detected in the radio band.
C1 [Laurent, P.] Commissariat Energie Atom & Energies Alternat, Inst Rech Lois Fondamentales Univers CEA IRFU, F-75205 Paris 13, France.
[Rodriguez, J.] Univ Paris Diderot, Inst Natl Sci Univers, CEA Saclay, DSM,IRFU,SAp,CEA,Lab AIM,CNRS, F-91191 Gif Sur Yvette, France.
[Wilms, J.; Grinberg, V.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
[Bel, M. Cadolle] European Space Astron Ctr, Sci Operat Dept, Int Gamma Ray Astrophys Lab INTEGRAL Sci Operat C, E-28691 Madrid, Spain.
[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.
RP Laurent, P (reprint author), Commissariat Energie Atom & Energies Alternat, Inst Rech Lois Fondamentales Univers CEA IRFU, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
EM plaurent@cea.fr
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468
FU European Commission [ITN 215212]; Bundesministerium fur Wirtschaft und
Technologie under Deutsches Zentrum fur Luftund Raumfahrt [50 OR 1007];
NASA [NNX08AE84G, NNX08AY24G, NX09AT28G]
FX ISGRI has been realized and maintained in flight by CEA-Saclay/IRFU with
the support of Centre National d'Etudes Spatiales. Based on observations
with INTEGRAL, a European Space Agency (ESA) project with instruments
and science data center funded by ESA member states (especially the
Principal Investigator countries: Denmark, France, Germany, Italy,
Switzerland, and Spain), Czech Republic and Poland, and with the
participation of Russia and the United States. We acknowledge partial
funding from the European Commission under contract ITN 215212 "Black
Hole Universe" and from the Bundesministerium fur Wirtschaft und
Technologie under Deutsches Zentrum fur Luftund Raumfahrt grant 50 OR
1007. K. P. acknowledges support by NASA's INTEGRAL Guest Observer
grants NNX08AE84G, NNX08AY24G, and NX09AT28G. We thank S. Corbel for
useful comments.
NR 31
TC 97
Z9 97
U1 1
U2 4
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 APR 22
PY 2011
VL 332
IS 6028
BP 438
EP 439
DI 10.1126/science.1200848
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 753NG
UT WOS:000289784900035
PM 21436402
ER
PT J
AU Minazzoli, O
Chauvineau, B
AF Minazzoli, Olivier
Chauvineau, Bertrand
TI Scalar-tensor propagation of light in the inner solar system including
relevant c(-4) contributions for ranging and time transfer
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID COSMOLOGICAL CONSTANT; GENERAL-RELATIVITY; SITTER SPACETIMES;
GRAVITY-FIELD; CORE; KERR-(ANTI); DYNAMICS; ROTATION; ORBITS; MODES
AB In a recent paper (Minazzoli and Chauvineau 2009 Phys. Rev. D 79 084027), motivated by forthcoming space experiments involving propagation of light in the solar system, we have proposed an extension of the IAU metric equations at the c(-4) level in general relativity. However, scalar-tensor theories may induce corrections numerically comparable to the c(-4) general relativistic terms. Accordingly, one first proposes in this paper an extension of Minazzoli and Chauvineau (2009) to the scalar-tensor case. The case of a hierarchized system (such as the solar system) is emphasized. In this case, the relevant metric solution is proposed. Then, the corresponding isotropic geodesic solution relevant for distance measurements and time transfers in the inner solar system is given in explicit form.
C1 [Minazzoli, Olivier; Chauvineau, Bertrand] Observ Cote Azur, ARTEMIS CNRS UMR 6162, UNS, F-06304 Nice, France.
[Minazzoli, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Minazzoli, Olivier] Univ Nice, ICRAnet, F-06103 Nice, France.
[Chauvineau, Bertrand] Observ Cote Azur, CASSIOPEE CNRS UMR6202, UNS, F-06304 Nice, France.
RP Minazzoli, O (reprint author), Observ Cote Azur, ARTEMIS CNRS UMR 6162, UNS, F-06304 Nice, France.
EM olivier.l.minazzoli@jpl.nasa.gov; bertrand.chauvineau@oca.eu
OI Minazzoli, Olivier/0000-0002-3151-7593
FU Government of the Principality of Monaco
FX OM wants to thank the Government of the Principality of Monaco for their
financial support.
NR 59
TC 15
Z9 15
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD APR 21
PY 2011
VL 28
IS 8
AR 085010
DI 10.1088/0264-9381/28/8/085010
PG 27
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 752FV
UT WOS:000289677400011
ER
PT J
AU Comiso, JC
Kwok, R
Martin, S
Gordon, AL
AF Comiso, Josefino C.
Kwok, Ronald
Martin, Seelye
Gordon, Arnold L.
TI Variability and trends in sea ice extent and ice production in the Ross
Sea
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SOUTHERN-OCEAN; CLIMATE-CHANGE; ANNULAR MODE; SHELF; THICKNESS; POLYNYA;
SURFACE; WESTERN; FLUX; OSCILLATION
AB Salt release during sea ice formation in the Ross Sea coastal regions is regarded as a primary forcing for the regional generation of Antarctic Bottom Water. Passive microwave data from November 1978 through 2008 are used to examine the detailed seasonal and interannual characteristics of the sea ice cover of the Ross Sea and the adjacent Bellingshausen and Amundsen seas. For this period the sea ice extent in the Ross Sea shows the greatest increase of all the Antarctic seas. Variability in the ice cover in these regions is linked to changes in the Southern Annular Mode and secondarily to the Antarctic Circumpolar Wave. Over the Ross Sea shelf, analysis of sea ice drift data from 1992 to 2008 yields a positive rate of increase in the net ice export of about 30,000 km(2) yr(-1). For a characteristic ice thickness of 0.6 m, this yields a volume transport of about 20 km(3) yr(-1), which is almost identical, within error bars, to our estimate of the trend in ice production. The increase in brine rejection in the Ross Shelf Polynya associated with the estimated increase with the ice production, however, is not consistent with the reported Ross Sea salinity decrease. The locally generated sea ice enhancement of Ross Sea salinity may be offset by an increase of relatively low salinity of the water advected into the region from the Amundsen Sea, a consequence of increased precipitation and regional glacial ice melt.
C1 [Comiso, Josefino C.] NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Martin, Seelye] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA.
[Gordon, Arnold L.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
RP Comiso, JC (reprint author), NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 614-1, Greenbelt, MD 20771 USA.
EM josefino.c.comiso@nasa.gov
RI Gordon, Arnold/H-1049-2011; Kwok, Ron/A-9762-2008
OI Gordon, Arnold/0000-0001-6480-6095; Kwok, Ron/0000-0003-4051-5896
FU NASA [NNG04GM69G]; National Science Foundation Office of the Polar
Programs [ANT-0538148]; National Science Foundation
FX J.C.C. would like to thank Robert Gerstein for programming support in
the analysis of SSM/I and AMSR-E data and is grateful to the NASA
Cryospheric Sciences Program for funding support. S. M. thanks Robert
Drucker for his help with Figure 13 and gratefully acknowledges the
support of NASA under contract NNG04GM69G. R. K. performed this work at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. A.L.G.'s support is from the National Science
Foundation Office of the Polar Programs grant ANT-0538148,
Lamont-Doherty contribution number 7397. We all thank the National Snow
and Ice Data Center for provision of the SMMR, SSM/I and AMSR-E data.
The ECMWF meteorological products are provided by the Data Support
Section of the Scientific Computing Division of the National Center for
Atmospheric Research (NCAR). NCAR is supported by grants from the
National Science Foundation.
NR 49
TC 60
Z9 60
U1 2
U2 34
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 APR 21
PY 2011
VL 116
AR C04021
DI 10.1029/2010JC006391
PG 19
WC Oceanography
SC Oceanography
GA 754JV
UT WOS:000289851800002
ER
PT J
AU Pryor, WR
Rymer, AM
Mitchell, DG
Hill, TW
Young, DT
Saur, J
Jones, GH
Jacobsen, S
Cowley, SWH
Mauk, BH
Coates, AJ
Gustin, J
Grodent, D
Gerard, JC
Lamy, L
Nichols, JD
Krimigis, SM
Esposito, LW
Dougherty, MK
Jouchoux, AJ
Stewart, AIF
McClintock, WE
Holsclaw, GM
Ajello, JM
Colwell, JE
Hendrix, AR
Crary, FJ
Clarke, JT
Zhou, XY
AF Pryor, Wayne R.
Rymer, Abigail M.
Mitchell, Donald G.
Hill, Thomas W.
Young, David T.
Saur, Joachim
Jones, Geraint H.
Jacobsen, Sven
Cowley, Stan W. H.
Mauk, Barry H.
Coates, Andrew J.
Gustin, Jacques
Grodent, Denis
Gerard, Jean-Claude
Lamy, Laurent
Nichols, Jonathan D.
Krimigis, Stamatios M.
Esposito, Larry W.
Dougherty, Michele K.
Jouchoux, Alain J.
Stewart, A. Ian F.
McClintock, William E.
Holsclaw, Gregory M.
Ajello, Joseph M.
Colwell, Joshua E.
Hendrix, Amanda R.
Crary, Frank J.
Clarke, John T.
Zhou, Xiaoyan
TI The auroral footprint of Enceladus on Saturn
SO NATURE
LA English
DT Article
ID IO FLUX TUBE; CASSINI; ATMOSPHERE; MAGNETOSPHERE; SPECTROMETER; JUPITER;
ORIGIN; PLASMA; PLUME
AB Although there are substantial differences between the magnetospheres of Jupiter and Saturn, it has been suggested that cryovolcanic activity at Enceladus(1-9) could lead to electrodynamic coupling between Enceladus and Saturn like that which links Jupiter with Io, Europa and Ganymede. Powerful field-aligned electron beams associated with the Io-Jupiter coupling, for example, create an auroral footprint in Jupiter's ionosphere(10,11). Auroral ultraviolet emission associated with Enceladus-Saturn coupling is anticipated to be just a few tenths of a kilorayleigh (ref. 12), about an order of magnitude dimmer than Io's footprint and below the observable threshold, consistent with its non-detection(13). Here we report the detection of magnetic-field-aligned ion and electron beams (offset several moon radii downstream from Enceladus) with sufficient power to stimulate detectable aurora, and the subsequent discovery of Enceladus-associated aurora in a few per cent of the scans of the moon's footprint. The footprint varies in emission magnitude more than can plausibly be explained by changes in magnetospheric parameters-and as such is probably indicative of variable plume activity.
C1 [Rymer, Abigail M.; Mitchell, Donald G.; Mauk, Barry H.; Krimigis, Stamatios M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Pryor, Wayne R.] Cent Arizona Coll, Dept Sci, Coolidge, AZ 85128 USA.
[Pryor, Wayne R.] Space Environm Technol, Pacific Palisades, CA 90272 USA.
[Hill, Thomas W.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Young, David T.; Crary, Frank J.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA.
[Saur, Joachim; Jacobsen, Sven] Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany.
[Jones, Geraint H.; Coates, Andrew J.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England.
[Jones, Geraint H.] Univ London Birkbeck Coll, Ctr Planetary Sci, London WC1E 6BT, England.
[Cowley, Stan W. H.; Nichols, Jonathan D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Gustin, Jacques; Grodent, Denis; Gerard, Jean-Claude] Univ Liege, Lab Phys Atmospher & Planetaire, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium.
[Lamy, Laurent] Univ Paris Diderot, Univ Pierre & Marie Curie, Lab Etud Spatiales & Instrumentat Astrophys, Observ Paris,Ctr Natl Rech Sci, F-92195 Meudon, France.
[Krimigis, Stamatios M.] Acad Athens, Athens 11527, Greece.
[Esposito, Larry W.; Jouchoux, Alain J.; Stewart, A. Ian F.; McClintock, William E.; Holsclaw, Gregory M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Dougherty, Michele K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Ajello, Joseph M.; Hendrix, Amanda R.; Zhou, Xiaoyan] Jet Prop Lab, Pasadena, CA 91109 USA.
[Colwell, Joshua E.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Clarke, John T.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
RP Rymer, AM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM abigail.rymer@jhuapl.edu
RI Nichols, Jonathan/F-5764-2010; Coates, Andrew/C-2396-2008; Clarke,
John/C-8644-2013; Jacobsen, Sven/E-1763-2013; Jones,
Geraint/C-1682-2008; Mauk, Barry/E-8420-2017;
OI Nichols, Jonathan/0000-0002-8004-6409; Coates,
Andrew/0000-0002-6185-3125; Mauk, Barry/0000-0001-9789-3797; Jones,
Geraint/0000-0002-5859-1136; GERARD, Jean-Claude/0000-0002-8565-8746
FU NASA/ESA; NASA
FX We acknowledge support from the NASA/ESA Cassini Project and NASA's
Cassini Data Analysis Program.
NR 30
TC 49
Z9 49
U1 0
U2 16
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 APR 21
PY 2011
VL 472
IS 7343
BP 331
EP 333
DI 10.1038/nature09928
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 752VW
UT WOS:000289724600035
PM 21512570
ER
PT J
AU Green, JD
Evans, NJ
Kospal, A
van Kempen, TA
Herczeg, G
Quanz, SP
Henning, T
Lee, JE
Dunham, MM
Meeus, G
Bouwman, J
van Dishoeck, E
Chen, JH
Gudel, M
Skinner, SL
Merello, M
Pooley, D
Rebull, LM
Guieu, S
AF Green, Joel D.
Evans, Neal J., II
Kospal, Agnes
van Kempen, Tim A.
Herczeg, Gregory
Quanz, Sascha P.
Henning, Thomas
Lee, Jeong-Eun
Dunham, Michael M.
Meeus, Gwendolyn
Bouwman, Jeroen
van Dishoeck, Ewine
Chen, Jo-Hsin
Guedel, Manuel
Skinner, Stephen L.
Merello, Manuel
Pooley, David
Rebull, Luisa M.
Guieu, Sylvain
TI DISENTANGLING THE ENVIRONMENT OF THE FU ORIONIS CANDIDATE HBC 722 WITH
HERSCHEL
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: jets and outflows; stars: individual (HBC 722); stars: pre-main
sequence; stars: variables: T Tauri, Herbig Ae/Be; submillimeter: ISM
ID NORTH-AMERICA; SHARC-II; SUBMILLIMETER; OBJECTS; STARS; EVOLUTION;
DISKS; DUST; PROTOSTELLAR; INSTRUMENT
AB We analyze the submillimeter emission surrounding the new FU Orionis-type object, HBC 722. We present the first epoch of observations of the active environs of HBC 722, with imaging and spectroscopy from PACS, SPIRE, and HIFI on board the Herschel Space Observatory, as well as CO J = 2-1 and 350 mu m imaging (SHARC-II) with the Caltech Submillimeter Observatory. The primary source of submillimeter continuum emission in the region-2MASS 20581767+4353310-is located 16 '' south-southeast of the optical flaring source while the optical and near-infrared emission is dominated by HBC 722. A bipolar outflow extends over HBC 722; the most likely driver is the submillimeter source. We detect warm (100 K) and hot (246 K) CO emission in the surrounding region, evidence of outflow-driven heating in the vicinity. The region around HBC 722 itself shows little evidence of heating driven by the new outbursting source itself.
C1 [Green, Joel D.; Evans, Neal J., II; Merello, Manuel; Pooley, David] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Kospal, Agnes; van Kempen, Tim A.; van Dishoeck, Ewine] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Kempen, Tim A.] Joint ALMA Off, Santiago, Chile.
[Herczeg, Gregory; van Dishoeck, Ewine] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany.
[Quanz, Sascha P.] ETH, Inst Astron, CH-8092 Zurich, Switzerland.
[Henning, Thomas; Bouwman, Jeroen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Gyeonggi 446701, South Korea.
[Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Meeus, Gwendolyn] Univ Autonoma Madrid, Dept Fis Teor C XV, E-28049 Madrid, Spain.
[Chen, Jo-Hsin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Guedel, Manuel] Univ Vienna, Dept Astron, A-1010 Vienna, Austria.
[Skinner, Stephen L.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Pooley, David] Eureka Sci, Austin, TX USA.
[Rebull, Luisa M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Guieu, Sylvain] European So Observ, Santiago 19, Chile.
RP Green, JD (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
RI Lee , Jeong-Eun/E-2387-2013; Guedel, Manuel/C-8486-2015;
OI Guedel, Manuel/0000-0001-9818-0588; Rebull, Luisa/0000-0001-6381-515X;
Herczeg, Gregory/0000-0002-7154-6065
FU Netherlands Organisation for Scientific Research; Ministry of Education,
Science and Technology [2010-0008704]
FX The authors acknowledge the Herschel Director, G.L. Pilbratt, for the
timely approval and execution of this Target of Opportunity program;
Amanda Heiderman for providing CSO data; Paul Harvey, Michelle Rascati,
and the HSC and NHSC Helpdesk for data processing and analysis
assistance, and Colette Salyk and Geoff Blake for helpful discussions.
The research of A.K. is supported by the Netherlands Organisation for
Scientific Research. The research of J.-E.L. is supported by Basic
Science Research Program through the National Research Foundation of
Korea (NRF) funded by the Ministry of Education, Science and Technology
(no. 2010-0008704). This work is based in part on data obtained as part
of the UKIRT Infrared Deep Sky Survey.
NR 34
TC 14
Z9 14
U1 1
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 APR 20
PY 2011
VL 731
IS 2
AR L25
DI 10.1088/2041-8205/731/2/L25
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797LB
UT WOS:000293128100004
ER
PT J
AU Brower, LP
Williams, EH
Fink, LS
Slayback, DA
Ramirez, MI
Garcia, MV
Zubieta, RR
Weiss, SB
Calvert, WH
Zuchowski, W
AF Brower, Lincoln P.
Williams, Ernest H.
Fink, Linda S.
Slayback, Daniel A.
Isabel Ramirez, M.
Van Limon Garcia, M.
Zubieta, Raul R.
Weiss, Stuart B.
Calvert, William H.
Zuchowski, Willow
TI OVERWINTERING CLUSTERS OF THE MONARCH BUTTERFLY COINCIDE WITH THE LEAST
HAZARDOUS VERTICAL TEMPERATURES IN THE OYAMEL FOREST
SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY
LA English
DT Article
DE Danaus plexippus; conservation; Monarch Butterfly Biosphere Reserve;
forest management; microclimate; trunk and bough clustering behavior;
vertical temperature distribution; negative effects of forest thinning
ID MOUNTAIN CHICKADEES; DANAUS-PLEXIPPUS; SITE SELECTION; MEXICO;
MICROCLIMATE; ADVANTAGES; SURVIVAL
AB During winter, monarch butterflies form dense colonies in oyamel fir forests on high mountains in central Mexico, where the forest canopy serves both as a blanket, moderating temperature, and an umbrella, shielding the butterflies from rain. In this study we investigated die vertical dimension of the butterflies' use of the oyamel forest: we predicted that clusters form at the heights above ground that provide the greatest protection from freezing. By suspending temperature recorders at eight heights, from ground level up to 22m, we established two vertical transects in the forest. We set one transect in a densely forested area and the other in a thinned area, and we recorded hourly temperatures from Jan 13 through Feb 5, 2006. Intermediate heights in the forest, from 10 to 15m above ground, remained the warmest during the cold night and early morning. We also determined that this temperature distribution matched available records of the vertical distribution of butterflies roosting in branch and trunk clusters. The vertical temperature profiles became uniform during mid-day. Temperature extremes were moderated more dining clear than during cloudy periods and more in the denser than in the thinned forest. Our results illustrate how the monarch butterfly is behaviorally adapted to the three-dimensional complexity of microclimate in the yarned forest. A denser forest provides better protection for the overwintering survival of monarch butterflies than a thinned forest. This research bolsters our other microclimatic studies, all of which point to the urgency of prohibiting logging within the oyamel forest used as wintering habitat by monarch butterflies.
C1 [Brower, Lincoln P.; Fink, Linda S.] Sweet Briar Coll, Dept Biol, Sweet Briar, VA 24595 USA.
[Williams, Ernest H.] Hamilton Coll, Dept Biol, Clinton, NY 13323 USA.
[Slayback, Daniel A.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Isabel Ramirez, M.] Univ Nacl Autonoma Mexico, Ctr Invest Geog Ambiental, Morelia 58190, Michoacan, Mexico.
[Van Limon Garcia, M.] Univ Nacl Autonoma Mexico, Fac Ciencias, Inst Geog, Mexico City 04510, DF, Mexico.
[Weiss, Stuart B.] Creekside Ctr Earth Observat, Menlo Pk, CA 94025 USA.
RP Brower, LP (reprint author), Sweet Briar Coll, Dept Biol, Sweet Briar, VA 24595 USA.
EM brower@sbc.edu
RI Slayback, Daniel/E-7465-2011; Ramirez, M. Isabel/D-3010-2012
FU National Science Foundation [14265, DEB-0415340]; Hamilton College;
DGAPA-PAPIIT [IN114707]
FX We are indebted to Prof. Rudolf Geiger for his pioneering syntheses of
microclimate. We thank Jennifer Wiley and Carlos Carrillo Tellez for
help in setting the vertical transects. We are grateful to lug.
Concepcion Miguel Martinez, former Director of the Monarch Butterfly
Biosphere Reserve, for facilitating our access to the study area, and to
the Arizmendi family for providing accommodations in Angangueo. We are
grateful to Myron Zalucki and Jenny Williams for critiques of the
manuscript and to Zach Dietz for extensive advice on statistical
analyses. Support during the 1978-1979 overwintering season was provided
by National Science Foundation grant 14265 to Amherst College with L.P.
Brower as principal investigator, and during 2006 by NSF grant
DEB-0415340 to Sweet Briar College with L.P. Brower and L.S. Fink as
principal investigators. We are grateful for additional support from the
October Hill Foundation, the Monarch Butterfly Sanctuary Foundation, and
SCION Natural Science Association, Ernest Williams was supported by the
Leonard C. Ferguson and Christian A. Johnson Professorship Funds at
Hamilton College. DGAPA-PAPIIT (IN114707) provided financial support to
M. Isabel Ramirez.
NR 62
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PU LEPIDOPTERISTS SOC
PI LOS ANGELES
PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA
SN 0024-0966
J9 J LEPID SOC
JI J. Lepid. Soc.
PD APR 20
PY 2011
VL 65
IS 1
BP 27
EP 46
PG 20
WC Entomology
SC Entomology
GA 758AM
UT WOS:000290131800003
ER
PT J
AU Foley, RJ
Andersson, K
Bazin, G
de Haan, T
Ruel, J
Ade, PAR
Aird, KA
Armstrong, R
Ashby, MLN
Bautz, M
Benson, BA
Bleem, LE
Bonamente, M
Brodwin, M
Carlstrom, JE
Chang, CL
Clocchiatti, A
Crawford, TM
Crites, AT
Desai, S
Dobbs, MA
Dudley, JP
Fazio, GG
Forman, WR
Garmire, G
George, EM
Gladders, MD
Gonzalez, AH
Halverson, NW
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Murray, SS
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruhl, JE
Saliwanchik, BR
Saro, A
Schaffer, KK
Shaw, L
Shirokoff, E
Song, J
Spieler, HG
Stalder, B
Stanford, SA
Staniszewski, Z
Stark, AA
Story, K
Stubbs, CW
Vanderlinde, K
Vieira, JD
Vikhlinin, A
Williamson, R
Zenteno, A
AF Foley, R. J.
Andersson, K.
Bazin, G.
de Haan, T.
Ruel, J.
Ade, P. A. R.
Aird, K. A.
Armstrong, R.
Ashby, M. L. N.
Bautz, M.
Benson, B. A.
Bleem, L. E.
Bonamente, M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Clocchiatti, A.
Crawford, T. M.
Crites, A. T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Fazio, G. G.
Forman, W. R.
Garmire, G.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
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.
Lueker, M.
Luong-Van, D.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruhl, J. E.
Saliwanchik, B. R.
Saro, A.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Song, J.
Spieler, H. G.
Stalder, B.
Stanford, S. A.
Staniszewski, Z.
Stark, A. A.
Story, K.
Stubbs, C. W.
Vanderlinde, K.
Vieira, J. D.
Vikhlinin, A.
Williamson, R.
Zenteno, A.
TI DISCOVERY AND COSMOLOGICAL IMPLICATIONS OF SPT-CL J2106-5844, THE MOST
MASSIVE KNOWN CLUSTER AT z > 1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE early universe; galaxies: clusters: individual (SPT-CL J2106-5844);
galaxies: evolution; galaxies: formation; large-scale structure of
universe
ID SOUTH-POLE TELESCOPE; IRAC SHALLOW SURVEY; GALAXY CLUSTER; X-RAY;
SPECTROSCOPIC CONFIRMATION; VELOCITY DISPERSIONS; ENVIRONMENT;
EXTRACTION; PRECISION; REDSHIFTS
AB Using the South Pole Telescope (SPT), we have discovered the most massive known galaxy cluster at z > 1, SPT-CL J2106-5844. In addition to producing a strong Sunyaev-Zel'dovich (SZ) effect signal, this system is a luminous X-ray source and its numerous constituent galaxies display spatial and color clustering, all indicating the presence of a massive galaxy cluster. Very Large Telescope and Magellan spectroscopy of 18 member galaxies shows that the cluster is at z = 1.132(-0.003)(+0.002). Chandra observations obtained through a combined HRC-ACIS GTO program reveal an X-ray spectrum with an Fe K line redshifted by z = 1.18 +/- 0.03. These redshifts are consistent with the galaxy colors found in optical, near-infrared, and mid-infrared imaging. SPT-CL J2106-5844 displays extreme X-ray properties for a cluster having a core-excluded temperature of T-X = 11.0(-1.9)(+2.6) keV and a luminosity (within r(500)) of L-X(0.5-2.0 keV) = (13.9 +/- 1.0) x 10(44) erg s(-1). The combined mass estimate from measurements of the SZ effect and X-ray data is M-200 = (1.27 +/- 0.21) x 10(15) h(70)(-1) M-circle dot. The discovery of such amassive gravitationally collapsed system at high redshift provides an interesting laboratory for galaxy formation and evolution, and is a probe of extreme perturbations of the primordial matter density field. We discuss the latter, determining that, under the assumption of Lambda CDM cosmology with only Gaussian perturbations, there is only a 7% chance of finding a galaxy cluster similar to SPT-CL J2106-5844 in the 2500 deg(2) SPT survey region and that only one such galaxy cluster is expected in the entire sky.
C1 [Foley, R. J.; Ashby, M. L. N.; Brodwin, M.; Fazio, G. G.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Andersson, K.; Bazin, G.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Andersson, K.; Bautz, M.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Bazin, G.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Ruel, J.; Rest, A.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
[Armstrong, R.; Desai, S.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 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.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; 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.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bonamente, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Desai, S.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Garmire, G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; 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.
[Joy, M.] NASA, George C Marshall Space Flight Ctr, VP62, Dept Space Sci, Huntsville, AL 35812 USA.
[Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[McMahon, J. J.; Song, 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, Dept Phys, Cleveland, OH 44106 USA.
[Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rfoley@cfa.harvard.edu
RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015;
Holzapfel, William/I-4836-2015;
OI Stubbs, Christopher/0000-0003-0347-1724; 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, PHY-0114422, AST-1009012,
AST-1009649, MRI-0723073]; Kavli Foundation; Gordon and Betty Moore
Foundation; NASA [12800071, 12800088, NAS8-03060]; JPL/Caltech; Chandra
X-ray Observatory Center; NASA Office of Space Science; National
Sciences and Engineering Research Council of Canada; Canada Research
Chairs program; Canadian Institute for Advanced Research; Excellence
Cluster Universe; DFG [TR33]; Clay Fellowship; KICP Fellowship; W.M.
Keck Foundation; Pennsylvania State University [2834-MIT-SAO-4018];
Basal CATA PFB [06/09]; FONDAP [15010003]; Alfred P. Sloan Research
Fellowship; Smithsonian Institution; Brinson Foundation
FX The South Pole Telescope program is supported by the National Science
Foundation through grant ANT-0638937. 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. This work
is based in part on observations obtained with the Spitzer Space
Telescope (PID 60099), 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. Additional data were obtained with the 6.5 m Magellan
Telescopes located at the Las Campanas Observatory, Chile. Support for
X-ray analysis was provided by NASA through Chandra Project Numbers
12800071 and 12800088 issued by the Chandra X-ray Observatory Center,
which is operated by the Smithsonian Astrophysical Observatory for and
on behalf of NASA under contract NAS8-03060. Observations from VLT
programs 086.A-0741 and 286.A-5021 were included in this work. 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. Galaxy cluster research at Harvard is supported by NSF
grant AST-1009012. Galaxy cluster research at SAO is supported in part
by NSF grants AST-1009649 and MRI-0723073. 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. X-ray research at the CfA is supported through NASA
Contract NAS 8-03060. The Munich group acknowledges support from the
Excellence Cluster Universe and the DFG research program TR33. R.J.F. is
supported by a Clay Fellowship. B. A. B. is supported by a KICP
Fellowship, support for M. Brodwin was provided by the W.M. Keck
Foundation, M. Bautz acknowledges support from contract
2834-MIT-SAO-4018 from the Pennsylvania State University to the
Massachusetts Institute of Technology. A.C. acknowledges the support of
grants Basal CATA PFB 06/09 and FONDAP No. 15010003. M.D. acknowledges
support from an Alfred P. Sloan Research Fellowship, W.F. and C.J.
acknowledge support from the Smithsonian Institution, and B.S.
acknowledges support from the Brinson Foundation.
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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 APR 20
PY 2011
VL 731
IS 2
AR 86
DI 10.1088/0004-637X/731/2/86
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600009
ER
PT J
AU Garcia, J
Kallman, TR
Mushotzky, RF
AF Garcia, J.
Kallman, T. R.
Mushotzky, R. F.
TI X-RAY REFLECTED SPECTRA FROM ACCRETION DISK MODELS. II. DIAGNOSTIC TOOLS
FOR X-RAY OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; atomic processes; black hole physics; line:
formation; radiative transfer; X-rays: general
ID RESONANT AUGER DESTRUCTION; K-SHELL PHOTOABSORPTION; ACTIVE GALACTIC
NUCLEI; COMPTON REFLECTION; SEYFERT-GALAXIES; ATOMIC DATABASE;
ALPHA-LINES; COLD MATTER; BLACK-HOLES; IRON
AB We present a comprehensive study of the emission spectra from accreting sources. We use our new reflection code to compute the reflected spectra from an accretion disk illuminated by X-rays. This set of models covers different values of ionization parameter, solar iron abundance, and photon index for the illuminating spectrum. These models also include the most complete and recent atomic data for the inner shell of the iron and oxygen isonuclear sequences. We concentrate our analysis on the 2-10 keV energy region and in particular on the iron K-shell emission lines. We show the dependency of the equivalent width (EW) of the Fe K alpha on the ionization parameter. The maximum value of the EW is similar to 800 eV for models with log xi similar to 1.5 and decreases monotonically as xi increases. For lower values of xi, the Fe K alpha EW decreases to a minimum near log xi similar to 0.8. We produce simulated CCD observations based on our reflection models. For low-ionized, reflection-dominated cases, the 2-10 keV energy region shows a very broad, curving continuum that cannot be represented by a simple power law. We show that in addition to the Fe K-shell emission, there are other prominent features such as the Si and S L alpha lines, a blend of Ar VIII-XI lines, and the Ca X K alpha line. In some cases, the S XV blends with the He-like Si radiative recombination continua producing a broad feature that cannot be reproduced by a simple Gaussian profile. This could be used as a signature of reflection.
C1 [Garcia, J.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Garcia, J.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mushotzky, R. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Garcia, J (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
EM javier.garcia@wmich.edu; timothy.r.kallman@nasa.gov;
richard@astro.umd.edu
FU NASA [05-ATP05-18]
FX This work was supported by a grant from the NASA astrophysics theory
program 05-ATP05-18. This research has made use of NASA's Astrophysics
Data System.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2011
VL 731
IS 2
AR 131
DI 10.1088/0004-637X/731/2/131
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600054
ER
PT J
AU Hickox, RC
Myers, AD
Brodwin, M
Alexander, DM
Forman, WR
Jones, C
Murray, SS
Brown, MJI
Cool, RJ
Kochanek, CS
Dey, A
Jannuzi, BT
Eisenstein, D
Assef, RJ
Eisenhardt, PR
Gorjian, V
Stern, D
Le Floc'h, E
Caldwell, N
Goulding, AD
Mullaney, JR
AF Hickox, Ryan C.
Myers, Adam D.
Brodwin, Mark
Alexander, David M.
Forman, William R.
Jones, Christine
Murray, Stephen S.
Brown, Michael J. I.
Cool, Richard J.
Kochanek, Christopher S.
Dey, Arjun
Jannuzi, Buell T.
Eisenstein, Daniel
Assef, Roberto J.
Eisenhardt, Peter R.
Gorjian, Varoujan
Stern, Daniel
Le Floc'h, Emeric
Caldwell, Nelson
Goulding, Andrew D.
Mullaney, James R.
TI CLUSTERING OF OBSCURED AND UNOBSCURED QUASARS IN THE BOOTES FIELD:
PLACING RAPIDLY GROWING BLACK HOLES IN THE COSMIC WEB
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; large-scale structure of universe; quasars: general;
surveys
ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; LUMINOUS RED GALAXIES;
DARK-MATTER HALOES; PHOTOMETRICALLY CLASSIFIED QUASARS; SPECTRAL
ENERGY-DISTRIBUTIONS; CROSS-CORRELATION FUNCTION; LARGE-SCALE STRUCTURE;
IRAC SHALLOW SURVEY; QSO REDSHIFT SURVEY
AB We present the first measurement of the spatial clustering of mid-infrared-selected obscured and unobscured quasars, using a sample in the redshift range 0.7 < z < 1.8 selected from the 9 deg(2) Bootes multiwavelength survey. Recently, the Spitzer Space Telescope and X-ray observations have revealed large populations of obscured quasars that have been inferred from models of the X-ray background and supermassive black hole evolution. To date, little is known about obscured quasar clustering, which allows us to measure the masses of their host dark matter halos and explore their role in the cosmic evolution of black holes and galaxies. In this study, we use a sample of 806 mid-infrared-selected quasars and approximate to 250,000 galaxies to calculate the projected quasar-galaxy cross-correlation function w(p) (R). The observed clustering yields characteristic dark matter halo masses of log(M-halo [h(-1) M-circle dot]) = 12.7(-0.6)(+0.4) and 13.3(-0.4)(+0.3) for unobscured quasars (QSO-1s) and obscured quasars (Obs-QSOs), respectively. The results for QSO-1s are in excellent agreement with previous measurements for optically selected quasars, while we conclude that the Obs-QSOs are at least as strongly clustered as the QSO-1s. We test for the effects of photometric redshift errors on the optically faint Obs-QSOs, and find that our method yields a robust lower limit on the clustering; photo-z errors may cause us to underestimate the clustering amplitude of the Obs-QSOs by at most similar to 20%. We compare our results to previous studies, and speculate on physical implications of stronger clustering for obscured quasars.
C1 [Hickox, Ryan C.; Alexander, David M.; Goulding, Andrew D.; Mullaney, James R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Hickox, Ryan C.; Brodwin, Mark; Forman, William R.; Jones, Christine; Murray, Stephen S.; Eisenstein, Daniel; Caldwell, Nelson; Goulding, Andrew D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Cool, Richard J.] Princeton Univ Observ, Princeton, NJ 08544 USA.
[Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Eisenstein, Daniel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Assef, Roberto J.; Eisenhardt, Peter R.; Gorjian, Varoujan; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Le Floc'h, Emeric; Mullaney, James R.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu CNRS, CE Saclay, F-91191 Gif Sur Yvette, France.
RP Hickox, RC (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
EM ryan.hickox@durham.ac.uk
RI Brown, Michael/B-1181-2015;
OI Brown, Michael/0000-0002-1207-9137; Alexander,
David/0000-0002-5896-6313; Forman, William/0000-0002-9478-1682
FU NOAO; STFC; SAO; NASA [NNX08AJ28G]
FX We thank our colleagues on the NDWFS, AGES, SDWFS, and XBootes teams. We
thank the anonymous referee for helpful comments that improved the
paper, and Philip Hopkins and Peder Norberg for productive discussions.
The NOAO Deep Wide-field Survey, and the research of A.D. and B.T.J. are
supported by NOAO, which is operated by the Association of Universities
for Research in Astronomy (AURA), Inc. under a cooperative agreement
with the National Science Foundation. This paper would not have been
possible without the efforts of the Chandra, Spitzer, KPNO, and MMT
support staff. Optical spectroscopy discussed in this paper was obtained
at the MMT Observatory, a joint facility of the Smithsonian Institution
and the University of Arizona. The first Spitzer MIPS survey of the
Bootes region was obtained using GTO time provided by the Spitzer
Infrared Spectrograph Team (PI: James Houck) and by M. Rieke. We thank
the collaborators in that work for access to the 24 micron catalog
generated from those data. R.C.H. was supported by an STFC Postdoctoral
Fellowship and an SAO Postdoctoral Fellowship, and A.D.M. was generously
funded by the NASA ADAP program under grant NNX08AJ28G. D.M.A. is
grateful to the Royal Society and Philip Leverhulme Prize for their
generous support. R.J.A. was supported by the NASA Postdoctoral Program,
administered by Oak Ridge Associated Universities through a contract
with NASA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2011
VL 731
IS 2
AR 117
DI 10.1088/0004-637X/731/2/117
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600040
ER
PT J
AU Kamenetzky, J
Glenn, J
Maloney, PR
Aguirre, JE
Bock, JJ
Bradford, CM
Earle, L
Inami, H
Matsuhara, H
Murphy, EJ
Naylor, BJ
Nguyen, HT
Zmuidzinas, J
AF Kamenetzky, J.
Glenn, J.
Maloney, P. R.
Aguirre, J. E.
Bock, J. J.
Bradford, C. M.
Earle, L.
Inami, H.
Matsuhara, H.
Murphy, E. J.
Naylor, B. J.
Nguyen, H. T.
Zmuidzinas, J.
TI THE DENSE MOLECULAR GAS IN THE CIRCUMNUCLEAR DISK OF NGC 1068
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 1068); galaxies: ISM; galaxies: Seyfert; ISM:
molecules
ID ACTIVE GALACTIC NUCLEUS; STAR-FORMATION; GALAXY NUCLEI; NGC-1068;
EMISSION; HCN; CO; SPECTROSCOPY; CHEMISTRY; LINE
AB We present a 190-307 GHz broadband spectrum obtained with Z-Spec of NGC 1068 with new measurements of molecular rotational transitions. After combining our measurementswith those previously published and considering the specific geometry of this Seyfert 2 galaxy, we conduct amulti-species Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+. We find that these molecules trace warm (T > 100 K) gas of H-2 number densities 10(4.2)-10(4.9) cm(-3). Our models also place strong constraints on the column densities and relative abundances of these molecules, as well as on the total mass in the circumnuclear disk. Using the uniform calibration afforded by the broad Z-Spec bandpass, we compare our line ratios to X-ray-dominated region (XDR) and photon-dominated region models. The majority of our line ratios are consistent with the XDR models at the densities indicated by the likelihood analysis, lending substantial support to the emerging interpretation that the energetics in the circumnuclear disk of NGC 1068 are dominated by accretion onto an active galactic nucleus.
C1 [Kamenetzky, J.; Glenn, J.; Maloney, P. R.; Earle, L.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA.
[Aguirre, J. E.] Univ Penn, Dept Phys, Philadelphia, PA 19104 USA.
[Bock, J. J.; Bradford, C. M.; Naylor, B. J.; Nguyen, H. T.; Zmuidzinas, J.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Earle, L.] Natl Renewable Energy Lab, Golden, CO 80401 USA.
[Inami, H.; Matsuhara, H.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Murphy, E. J.] Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
RP Kamenetzky, J (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389-UCB, Boulder, CO 80303 USA.
OI Kamenetzky, Julia/0000-0001-7877-7942
FU NASA [NAGS-11911, NAGS-12788]; NSF [AST-0239270, AST-087990]; Research
Corporation Award [RI0928]; Caltech Millikan fellowship; JPL Director's
fellowship; NRAO
FX We thank the anonymous referee for a thorough and constructive report,
and we also express our gratitude to the staff at the Caltech
Submillimeter Observatory. We acknowledge the following grants and
fellowships in support of this work: NASA SARA grants NAGS-11911 and
NAGS-12788, an NSF Career grant AST-0239270, and a Research Corporation
Award RI0928 to J.G.; a Caltech Millikan fellowship and JPL Director's
fellowship to C.M.B.; an NRAO Jansky fellowship and NSF grant AST-087990
to J.E.A.; a NASA GSRP fellowship to L.E.; and an NSF GRFP fellowship to
J.K.
NR 46
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U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2011
VL 731
IS 2
AR 83
DI 10.1088/0004-637X/731/2/83
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600006
ER
PT J
AU Linker, JA
Lionello, R
Mikic, Z
Titov, VS
Antiochos, SK
AF Linker, Jon A.
Lionello, Roberto
Mikic, Zoran
Titov, Viacheslav S.
Antiochos, Spiro K.
TI THE EVOLUTION OF OPEN MAGNETIC FLUX DRIVEN BY PHOTOSPHERIC DYNAMICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); Sun: corona; Sun: magnetic topology; solar
wind
ID SLOW SOLAR-WIND; WHOLE SUN MONTH; CORONAL MASS EJECTIONS; DIFFERENTIAL
ROTATION; MAGNETOHYDRODYNAMIC SIMULATIONS; FIELD STRENGTH; MHD MODEL;
HOLES; INTERPLANETARY; SPEED
AB The coronal magnetic field is of paramount importance in solar and heliospheric physics. Two profoundly different views of the coronal magnetic field have emerged. In quasi-steady models, the predominant source of open magnetic field is in coronal holes. In contrast, in the interchange model, the open magnetic flux is conserved, and the coronal magnetic field can only respond to the photospheric evolution via interchange reconnection. In this view, the open magnetic flux diffuses through the closed, streamer belt fields, and substantial open flux is present in the streamer belt during solar minimum. However, Antiochos and coworkers, in the form of a conjecture, argued that truly isolated open flux cannot exist in a configuration with one heliospheric current sheet-it will connect via narrow corridors to the polar coronal hole of the same polarity. This contradicts the requirements of the interchange model. We have performed an MHD simulation of the solar corona up to 20 R-circle dot to test both the interchange model and the Antiochos conjecture. We use a synoptic map for Carrington rotation 1913 as the boundary condition for the model, with two small bipoles introduced into the region where a positive polarity extended coronal hole forms. We introduce flows at the photospheric boundary surface to see if open flux associated with the bipoles can be moved into the closed-field region. Interchange reconnection does occur in response to these motions. However, we find that the open magnetic flux cannot be simply injected into closed-field regions-the flux eventually closes down and disconnected flux is created. Flux either opens or closes, as required, to maintain topologically distinct open- and closed-field regions, with no indiscriminate mixing of the two. The early evolution conforms to the Antiochos conjecture in that a narrow corridor of open flux connects the portion of the coronal hole that is nearly detached by one of the bipoles. In the later evolution, a detached coronal hole forms, in apparent violation of the Antiochos conjecture. Further investigation reveals that this detached coronal hole is actually linked to the extended coronal hole by a separatrix footprint on the photosphere of zero width. Therefore, the essential idea of the conjecture is preserved, if we modify it to state that coronal holes in the same polarity region are always linked, either by finite width corridors or separatrix footprints. The implications of these results for interchange reconnection and the sources of the slow solar wind are briefly discussed.
C1 [Linker, Jon A.; Lionello, Roberto; Mikic, Zoran; Titov, Viacheslav S.] Predict Sci Inc, San Diego, CA 92121 USA.
[Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Linker, JA (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA.
EM linkerj@predsci.com; lionel@predsci.com; mikicz@predsci.com;
titovv@predsci.com; spiro.antiochos@nasa.gov
RI Antiochos, Spiro/D-4668-2012
OI Antiochos, Spiro/0000-0003-0176-4312
FU NASA; NSF; AFOSR; Center for Integrated Space Weather Modeling (an NSF
Science and Technology Center)
FX This work was supported by NASA's Heliophysics Theory, LWS, and Guest
Investigator programs, the LWS Strategic Capabilities Program (NASA,
NSF, and AFOSR), and the Center for Integrated Space Weather Modeling
(an NSF Science and Technology Center). Computational resources were
provided by the NSF supported Texas Advanced Computing Center (TACC) in
Austin and the NASA Advanced Supercomputing Division (NAS) at Ames
Research Center. This work was initiated and greatly benefitted from
discussions in the LWS TR&T focus team on the solar and heliospheric
magnetic field.
NR 77
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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 APR 20
PY 2011
VL 731
IS 2
AR 110
DI 10.1088/0004-637X/731/2/110
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600033
ER
PT J
AU Marriage, TA
Juin, JB
Lin, YT
Marsden, D
Nolta, MR
Partridge, B
Ade, PAR
Aguirre, P
Amiri, M
Appel, JW
Barrientos, LF
Battistelli, ES
Bond, JR
Brown, B
Burger, B
Chervenak, J
Das, S
Devlin, MJ
Dicker, SR
Doriese, WB
Dunkley, J
Dunner, R
Essinger-Hileman, T
Fisher, RP
Fowler, JW
Hajian, A
Halpern, M
Hasselfield, M
Hernandez-Monteagudo, C
Hilton, GC
Hilton, M
Hincks, AD
Hlozek, R
Huffenberger, KM
Hughes, DH
Hughes, JP
Infante, L
Irwin, KD
Kaul, M
Klein, J
Kosowsky, A
Lau, JM
Limon, M
Lupton, RH
Martocci, K
Mauskopf, P
Menanteau, F
Moodley, K
Moseley, H
Netterfield, CB
Niemack, MD
Page, LA
Parker, L
Quintana, H
Reid, B
Sehgal, N
Sherwin, BD
Sievers, J
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Trac, H
Tucker, C
Warne, R
Wilson, G
Wollack, E
Zhao, Y
AF Marriage, Tobias A.
Baptiste Juin, Jean
Lin, Yen-Ting
Marsden, Danica
Nolta, Michael R.
Partridge, Bruce
Ade, Peter A. R.
Aguirre, Paula
Amiri, Mandana
Appel, John William
Felipe Barrientos, L.
Battistelli, Elia S.
Bond, John R.
Brown, Ben
Burger, Bryce
Chervenak, Jay
Das, Sudeep
Devlin, Mark J.
Dicker, Simon R.
Doriese, W. Bertrand
Dunkley, Joanna
Duenner, Rolando
Essinger-Hileman, Thomas
Fisher, Ryan P.
Fowler, Joseph W.
Hajian, Amir
Halpern, Mark
Hasselfield, Matthew
Hernandez-Monteagudo, Carlos
Hilton, Gene C.
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Huffenberger, Kevin M.
Handel Hughes, David
Hughes, John P.
Infante, Leopoldo
Irwin, Kent D.
Kaul, Madhuri
Klein, Jeff
Kosowsky, Arthur
Lau, Judy M.
Limon, Michele
Lupton, Robert H.
Martocci, Krista
Mauskopf, Phil
Menanteau, Felipe
Moodley, Kavilan
Moseley, Harvey
Netterfield, Calvin B.
Niemack, Michael D.
Page, Lyman A.
Parker, Lucas
Quintana, Hernan
Reid, Beth
Sehgal, Neelima
Sherwin, Blake D.
Sievers, Jon
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Thornton, Robert
Trac, Hy
Tucker, Carole
Warne, Ryan
Wilson, Grant
Wollack, Ed
Zhao, Yue
TI THE ATACAMA COSMOLOGY TELESCOPE: EXTRAGALACTIC SOURCES AT 148 GHz IN THE
2008 SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; galaxies: active; radio continuum:
galaxies; surveys
ID SOUTH-POLE TELESCOPE; ZELDOVICH POWER SPECTRUM; GALAXY CLUSTERS; SOURCE
CATALOG; RADIO-SOURCES; SOURCE COUNTS; SKY SURVEY; ANISOTROPY; FIELD; SZ
AB We report on extragalactic sources detected in a 455 deg(2) map of the southern sky made with data at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. We provide a catalog of 157 sources with flux densities spanning two orders of magnitude: from 15 mJy to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low-redshift X-ray-selected galaxy clusters. Estimates of the radio to millimeter-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (> 50 mJy) 148 GHz selected sample with complete cross-identifications from the Australia Telescope 20 GHz survey, we observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha(5-20) = -0.07 +/- 0.06, alpha(20-148) = -0.39 +/- 0.04, and alpha(5-148) = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148 GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C-Sync = (2.8 +/- 0.3) x 10(-6) mu K-2.
C1 [Marriage, Tobias A.; Lin, Yen-Ting; Das, Sudeep; Dunkley, Joanna; Hajian, Amir; Lupton, Robert H.; Spergel, David N.; Trac, Hy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Baptiste Juin, Jean; Lin, Yen-Ting; Aguirre, Paula; Felipe Barrientos, L.; Duenner, Rolando; Infante, Leopoldo; Quintana, Hernan] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
[Marsden, Danica; Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Nolta, Michael R.; Bond, John R.; Hajian, Amir; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Appel, John William; Das, Sudeep; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Lau, Judy M.; Limon, Michele; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Doriese, W. Bertrand; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa.
[Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Handel Hughes, David] INAOE, Puebla, Mexico.
[Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Lau, Judy M.; Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Limon, Michele] Columbia Astrophys Lab, New York, NY 10027 USA.
[Martocci, Krista; Switzer, Eric R.] Lab Astrophys & Space Res, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Reid, Beth] Univ Barcelona, ICC, E-08028 Barcelona, Spain.
[Reid, Beth] Univ Barcelona, ICREA, E-08028 Barcelona, Spain.
[Thornton, Robert] W Chester Univ, Dept Phys, W Chester, PA 19383 USA.
[Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wilson, Grant] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP Marriage, TA (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew
James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Limon, Michele/0000-0002-5900-2698; Trac, Hy/0000-0001-6778-3861;
Wollack, Edward/0000-0002-7567-4451; Huffenberger,
Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534;
Sievers, Jonathan/0000-0001-6903-5074
FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768]; Princeton University; University of Pennsylvania; Canada
Foundation for Innovation under the auspices of Compute Canada;
Government of Ontario; Ontario Research Fund-Research Excellence;
University of Toronto; NASA [NNX08AH30G]; FONDECYT [3085031]; Natural
Science and Engineering Research Council of Canada (NSERC); NSF
[AST-0546035, AST-0606975]; FONDAP Centro de Astrofisica; U.S.
Department of Energy [DE-AC3-76SF00515]; CONICYT; MECESUP; Fundacion
Andes; Rhodes Trust; NSF Physics Frontier Center [PHY-0114422]; World
Premier International Research Center Initiative, MEXT, Japan
FX This work was supported by the U.S. National Science Foundation through
awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731,
and PIRE-0507768. Funding was also provided by Princeton University and
the University of Pennsylvania. The PIRE program made possible exchanges
between Chile, South Africa, Spain, and the US that enabled this
research program. Computations were performed on the GPC supercomputer
at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation
for Innovation under the auspices of Compute Canada; the Government of
Ontario; Ontario Research Fund-Research Excellence; and the University
of Toronto.; T.M. was supported through NASA grant NNX08AH30G. J.B.J.
was supported by the FONDECYT grant 3085031. A. D. H. received
additional support from a Natural Science and Engineering Research
Council of Canada (NSERC) PGS-D scholarship. A. K. and B. P. were
partially supported through NSF AST-0546035 and AST-0606975,
respectively, for work on ACT. H. Q. and L. I. acknowledge partial
support from FONDAP Centro de Astrofisica. N.S. is supported by the U.S.
Department of Energy contract to SLAC no. DE-AC3-76SF00515. R. D. was
supported by CONICYT, MECESUP, and Fundacion Andes. R. H. was supported
by the Rhodes Trust. E. S. acknowledges support by NSF Physics Frontier
Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics.
Y.T.L. acknowledges support from the World Premier International
Research Center Initiative, MEXT, Japan. The ACT data will be made
public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web
site (http://www.physics.princeton.edu/act/).
NR 48
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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 APR 20
PY 2011
VL 731
IS 2
AR 100
DI 10.1088/0004-637X/731/2/100
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600023
ER
PT J
AU Mullan, B
Konstantopoulos, S
Kepley, AA
Lee, KH
Charlton, JC
Knierman, K
Bastian, N
Chandar, R
Durrell, PR
Elmegreen, D
English, J
Gallagher, SC
Gronwall, C
Hibbard, JE
Hunsberger, S
Johnson, KE
Maybhate, A
Palma, C
Trancho, G
Vacca, WD
AF Mullan, B.
Konstantopoulos, S.
Kepley, A. A.
Lee, K. H.
Charlton, J. C.
Knierman, K.
Bastian, N.
Chandar, R.
Durrell, P. R.
Elmegreen, D.
English, J.
Gallagher, S. C.
Gronwall, C.
Hibbard, J. E.
Hunsberger, S.
Johnson, K. E.
Maybhate, A.
Palma, C.
Trancho, G.
Vacca, W. D.
TI STAR CLUSTERS IN THE TIDAL TAILS OF INTERACTING GALAXIES: CLUSTER
POPULATIONS ACROSS A VARIETY OF TAIL ENVIRONMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: interactions; galaxies: photometry; galaxies: star clusters:
general
ID YOUNG GLOBULAR-CLUSTERS; SPACE-TELESCOPE OBSERVATIONS; INITIAL MASS
FUNCTION; DWARF GALAXIES; STELLAR POPULATIONS; LUMINOSITY FUNCTION;
SPIRAL GALAXIES; PHOTOMETRIC EVOLUTION; SPATIAL-DISTRIBUTION; ANTENNAE
GALAXIES
AB We have searched for compact stellar structures within 17 tidal tails in 13 different interacting galaxies using F606W- and F814W-band images from the Wide Field Planetary Camera 2 on the Hubble Space Telescope. The sample of tidal tails includes a diverse population of optical properties, merging galaxy mass ratios, Hi content, and ages. Combining our tail sample with Knierman et al., we find evidence of star clusters formed in situ with M-V < -8.5 and V - I < 2.0 in 10 of 23 tidal tails; we are able to identify cluster candidates to M-V = -6.5 in the closest tails. Three tails offer clear examples of "beads on a string" star formation morphology in V - I color maps. Two tails present both tidal dwarf galaxy candidates and cluster candidates. Statistical diagnostics indicate that clusters in tidal tails may be drawn from the same power-law luminosity functions (with logarithmic slopes approximate to-2 to -2.5) found in quiescent spiral galaxies and interiors of interacting systems. We find that the tail regions with the largest number of observable clusters are relatively young (less than or similar to 250 Myr old) and bright (V less than or similar to 24 mag arcsec(-2)), probably attributed to the strong bursts of star formation in interacting systems soon after periapse. Otherwise, we find no statistical difference between cluster-rich and cluster-poor tails in terms of many observable characteristics, though this analysis suffers from complex, unresolved gas dynamics and projection effects.
C1 [Mullan, B.; Konstantopoulos, S.; Lee, K. H.; Charlton, J. C.; Gronwall, C.; Hunsberger, S.; Palma, C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16803 USA.
[Kepley, A. A.; Johnson, K. E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Kepley, A. A.; Hibbard, J. E.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Knierman, K.] Arizona State Univ, Bateman Phys Sci Ctr, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Bastian, N.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Chandar, R.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Durrell, P. R.] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA.
[Elmegreen, D.] Vassar Coll, Dept Phys & Astron, Poughkeepsie, NY 12604 USA.
[English, J.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada.
[Gallagher, S. C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Maybhate, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Trancho, G.] Gemini Observ, La Serena, Chile.
[Vacca, W. D.] NASA Ames Res Ctr, Univ Space Res Assoc, Stratospher Observ Infrared Astron, Stanford, CA 94305 USA.
RP Mullan, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16803 USA.
EM mullan@astro.psu.edu
OI Konstantopoulos, Iraklis/0000-0003-2177-0146
FU Space Telescope Science Institute [HST-GO-11134.05-A]
FX We wish to thank Barbel Koribalski for sharing Hi data and helpful
comments for NGC 6872. This project was supported by a grant from the
Space Telescope Science Institute (grant No. HST-GO-11134.05-A).
NR 113
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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 APR 20
PY 2011
VL 731
IS 2
AR 93
DI 10.1088/0004-637X/731/2/93
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600016
ER
PT J
AU Sandell, G
Weintraub, DA
Hamidouche, M
AF Sandell, Goeran
Weintraub, David A.
Hamidouche, Murad
TI A SUB-MILLIMETER MAPPING SURVEY OF HERBIG AeBe STARS (vol 26, pg 727,
2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Sandell, Goeran; Hamidouche, Murad] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Weintraub, David A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
RP Sandell, G (reprint author), NASA, SOFIA USRA, Ames Res Ctr, Mail Stop N211-3,Bldg N211,Rm 249, Moffett Field, CA 94035 USA.
NR 1
TC 1
Z9 1
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2011
VL 731
IS 2
AR 133
DI 10.1088/0004-637X/731/2/133
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600056
ER
PT J
AU Su, Y
Holman, GD
Dennis, BR
AF Su, Yang
Holman, Gordon D.
Dennis, Brian R.
TI EVIDENCE FOR THE FULL HARD X-RAY SPECTRAL SIGNATURE OF NONUNIFORM
IONIZATION IN A SOLAR FLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: chromosphere; Sun: flares; Sun: X-rays, gamma rays
ID THERMAL ELECTRONS; REVERSE-CURRENT; BREMSSTRAHLUNG; TARGET; ENERGY;
RHESSI; EXPLANATION; BURSTS; BEAMS
AB The hard X-ray (HXR) emission from solar flares is observed primarily from the footpoints of flare magnetic loops, where nonthermal electrons are understood to emit thick-target bremsstrahlung as they stream from the fully ionized hot corona to the denser, cooler, and partially ionized chromosphere. The change in the plasma ionization along the path of the electrons should result in a characteristic upward break and corresponding flattening of the X-ray spectrum with increasing energy at lower energies, and a downward break at higher energies. Due to the presence of thermal emission, the upward break usually cannot be observed. We report the first evidence for both breaks in spectra measured with the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) during the GOES X1.2 class flare that happened on 2002 October 31. The RHESSI X-ray spectral analysis shows both the breakup at similar to 49 keV and the breakdown at similar to 134 keV at the HXR peak time. The time evolution of both breaks also agrees with the nonuniform ionization (NUI) model. Other possible explanations for the breaks are considered, but the NUI model provides the simplest explanation for the spectral shape and its time evolution. We find that the average column density of the fully ionized plasma changed from 2 x 10(19) cm(-2) in the rise phase to 7 x 10(21) cm(-2) after the peak. This indicates that plasma in the target was heated and became ionized during the flare, in agreement with heating by the nonthermal electrons and chromospheric evaporation expected in the collisional thick-target model.
C1 [Su, Yang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Su, Yang; Holman, Gordon D.; Dennis, Brian R.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Su, Yang] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Peoples R China.
RP Su, Y (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM yang.su@nasa.gov; gordon.d.holman@nasa.gov
RI Dennis, Brian/C-9511-2012; Holman, Gordon/C-9548-2012; Su,
Yang/J-5381-2014
FU NSF [ATM-0725135]; NASA [NNX06AE64G]; National Natural Science
Foundation of China [10773031, 10833007, 11078025]; Ministry of Science
and Technology of China [MSTC 2011CB811402]; RHESSI
FX We thank the RHESSI PI team for the excellence and easy availability of
the data and the analysis software. Yang Su thanks Dr. Linhui Sui and
Dr. Jeffrey W. Brosius for providing the research opportunity, Qingrong
Chen and the referee for the valuable discussions and comments. Yang Su
also acknowledges NSF support through ATM-0725135 and NASA support
through grant NNX06AE64G. This work was supported in part by the
National Natural Science Foundation of China (grant nos. 10773031,
10833007, 11078025), the Ministry of Science and Technology of China
(MSTC 2011CB811402), the RHESSI Project, and a NASA HGI (Heliophysics
Guest Investigator) grant.
NR 25
TC 10
Z9 11
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2011
VL 731
IS 2
AR 106
DI 10.1088/0004-637X/731/2/106
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600029
ER
PT J
AU Titov, VS
Mikic, Z
Linker, JA
Lionello, R
Antiochos, SK
AF Titov, V. S.
Mikic, Z.
Linker, J. A.
Lionello, R.
Antiochos, S. K.
TI MAGNETIC TOPOLOGY OF CORONAL HOLE LINKAGES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun: corona; Sun: coronal mass ejections (CMEs); Sun:
magnetic topology
ID QUASI-SEPARATRIX LAYERS; SLOW SOLAR-WIND; MASS EJECTIONS; NULL POINTS;
ACTIVE REGIONS; RECONNECTION; FIELDS; MODEL; DYNAMICS; OUTFLOWS
AB In recent work, Antiochos and coworkers argued that the boundary between the open and closed field regions on the Sun can be extremely complex with narrow corridors of open flux connecting seemingly disconnected coronal holes from the main polar holes and that these corridors may be the sources of the slow solar wind. We examine, in detail, the topology of such magnetic configurations using an analytical source surface model that allows for analysis of the field with arbitrary resolution. Our analysis reveals three new important results. First, a coronal hole boundary can join stably to the separatrix boundary of a parasitic polarity region. Second, a single parasitic polarity region can produce multiple null points in the corona and, more important, separator lines connecting these points. It is known that such topologies are extremely favorable for magnetic reconnection, because they allow this process to occur over the entire length of the separators rather than being confined to a small region around the nulls. Finally, the coronal holes are not connected by an open-field corridor of finite width, but instead are linked by a singular line that coincides with the separatrix footprint of the parasitic polarity. We investigate how the topological features described above evolve in response to the motion of the parasitic polarity region. The implications of our results for the sources of the slow solar wind and for coronal and heliospheric observations are discussed.
C1 [Titov, V. S.; Mikic, Z.; Linker, J. A.; Lionello, R.] Predict Sci Inc, San Diego, CA 92121 USA.
[Antiochos, S. K.] NASA GSFC, Greenbelt, MD 20771 USA.
RP Titov, VS (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA.
EM titovv@predsci.com; mikicz@predsci.com; linkerj@predsci.com;
lionel@predsci.com; spiro.antiochos@nasa.gov
RI Antiochos, Spiro/D-4668-2012
OI Antiochos, Spiro/0000-0003-0176-4312
FU NASA; Center for Integrated Space Weather Modeling (an NSF Science and
Technology Center)
FX We thank the referee for a careful review of our paper, which helped us
to significantly improve the presentation of our results. The
contribution of V.S.T., Z.M., J.R.L., and R.L. was supported by NASA's
Heliophysics Theory, Living With a Star, and SR&T programs, and the
Center for Integrated Space Weather Modeling (an NSF Science and
Technology Center). The contribution by S.K.A. was supported by the NASA
HTP, TR&T, and SR&T programs.
NR 34
TC 38
Z9 38
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2011
VL 731
IS 2
AR 111
DI 10.1088/0004-637X/731/2/111
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600034
ER
PT J
AU Toma, K
Sakamoto, T
Meszaros, P
AF Toma, Kenji
Sakamoto, Takanori
Meszaros, Peter
TI POPULATION III GAMMA-RAY BURST AFTERGLOWS: CONSTRAINTS ON STELLAR MASSES
AND EXTERNAL MEDIUM DENSITIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; dark ages, reionization, first stars; gamma-ray
burst: general; radio continuum: general; stars: Population III;
surveys; X-rays: bursts
ID HIGH-REDSHIFT; BLACK-HOLES; COSMIC REIONIZATION; FERMI OBSERVATIONS;
RELATIVISTIC JETS; RADIO AFTERGLOWS; MAGNETIC-FIELDS; MASSIVE STARS;
NEUTRON-STARS; 1ST STAR
AB Population (Pop.) III stars are theoretically expected to be prominent around redshifts z similar to 20, consisting of mainly very massive stars with M-* greater than or similar to 100 M-circle dot, though there is no direct observational evidence for these objects. They may produce collapsar gamma-ray bursts (GRBs), with jets driven by magnetohydrodynamic processes, whose total isotropic-equivalent energy could be as high as E-iso greater than or similar to 10(57) erg over a cosmological-rest-frame duration of t(d) greater than or similar to 10(4) s, depending on the progenitor mass. Here, we calculate the afterglow spectra of such Pop. III GRBs based on the standard external shock model and show that they will be detectable with the Swift Burst Alert Telescope (BAT)/XRT and Fermi Large Area Telescope (LAT) instruments. We find that in some cases a spectral break due to electron-positron pair creation will be observable in the LAT energy range, which can put constraints on the ambient density of the pre-collapse Pop. III star. Thus, high-redshift GRB afterglow observations could be unique and powerful probes of the properties of Pop. III stars and their environments. We examine the trigger threshold of the BAT instrument in detail, focusing on the image trigger system, and show that the prompt emission of Pop. III GRBs could also be detected by BAT. Finally we briefly show that the late-time radio afterglows of Pop. III GRBs for typical parameters, despite the large distances, can be very bright: similar or equal to 140 mJy at 1 GHz, which may lead to a constraint on the Pop. III GRB rate from the current radio survey data, and similar or equal to 2.4 mJy at 70 MHz, which implies that Pop. III GRB radio afterglows could be interesting background source candidates for 21 cm absorption line detections.
C1 [Toma, Kenji; Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Toma, Kenji; Meszaros, Peter] Penn State Univ, Ctr Particle Astrophys, University Pk, PA 16802 USA.
[Sakamoto, Takanori] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, Takanori] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Meszaros, Peter] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
RP Toma, K (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM toma@astro.psu.edu; takanori@milkyway.gsfc.nasa.gov; nnp@astro.psu.edu
FU NASA [NNX09AT72G, NNX08AL40G]; NSF [PHY-0757155]
FX We thank D. N. Burrows, A. D. Falcone, D. B. Fox, A. Gal-Yam, S. Gao, K.
Murase, S. Naoz, and the anonymous referee for useful comments. We
acknowledge NASA NNX09AT72G, NASA NNX08AL40G, and NSF PHY-0757155 for
partial support.
NR 91
TC 47
Z9 47
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2011
VL 731
IS 2
AR 127
DI 10.1088/0004-637X/731/2/127
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600050
ER
PT J
AU Antiochos, SK
Mikic, Z
Titov, VS
Lionello, R
Linker, JA
AF Antiochos, S. K.
Mikic, Z.
Titov, V. S.
Lionello, R.
Linker, J. A.
TI A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun: corona; Sun: magnetic topology
ID HELIOSPHERIC PLASMA SHEET; OPEN MAGNETIC-FLUX; WHOLE SUN MONTH; CORONAL
STREAMERS; PHOTOSPHERIC NETWORK; RECONNECTION; DYNAMICS; FIELDS;
INTERPLANETARY; ACCELERATION
AB Models for the origin of the slow solar wind must account for two seemingly contradictory observations: the slow wind has the composition of the closed-field corona, implying that it originates from the continuous opening and closing of flux at the boundary between open and closed field. On the other hand, the slow wind also has large angular width, up to similar to 60 degrees, suggesting that its source extends far from the open-closed boundary. We propose a model that can explain both observations. The key idea is that the source of the slow wind at the Sun is a network of narrow (possibly singular) open-field corridors that map to a web of separatrices and quasi-separatrix layers in the heliosphere. We compute analytically the topology of an open-field corridor and show that it produces a quasi-separatrix layer in the heliosphere that extends to angles far from the heliospheric current sheet. We then use an MHD code and MDI/SOHO observations of the photospheric magnetic field to calculate numerically, with high spatial resolution, the quasi-steady solar wind, and magnetic field for a time period preceding the 2008 August 1 total solar eclipse. Our numerical results imply that, at least for this time period, a web of separatrices (which we term an S-web) forms with sufficient density and extent in the heliosphere to account for the observed properties of the slow wind. We discuss the implications of our S-web model for the structure and dynamics of the corona and heliosphere and propose further tests of the model.
C1 [Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mikic, Z.; Titov, V. S.; Lionello, R.; Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA.
RP Antiochos, SK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM spiro.antiochos@nasa.gov
RI Antiochos, Spiro/D-4668-2012
OI Antiochos, Spiro/0000-0003-0176-4312
FU NASA
FX This work has been supported by the NASA TR&T, SR&T, and HTP programs.
The work has benefited greatly from the authors' participation in the
NASA TR&T focused science team on the solar-heliospheric magnetic field.
S.K.A. thanks J. Karpen for invaluable scientific discussions and help
with the graphics.
NR 66
TC 71
Z9 71
U1 2
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2011
VL 731
IS 2
AR 112
DI 10.1088/0004-637X/731/2/112
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753MM
UT WOS:000289779600035
ER
PT J
AU Kondo, Y
Matsui, H
Moteki, N
Sahu, L
Takegawa, N
Kajino, M
Zhao, Y
Cubison, MJ
Jimenez, JL
Vay, S
Diskin, GS
Anderson, B
Wisthaler, A
Mikoviny, T
Fuelberg, HE
Blake, DR
Huey, G
Weinheimer, AJ
Knapp, DJ
Brune, WH
AF Kondo, Y.
Matsui, H.
Moteki, N.
Sahu, L.
Takegawa, N.
Kajino, M.
Zhao, Y.
Cubison, M. J.
Jimenez, J. L.
Vay, S.
Diskin, G. S.
Anderson, B.
Wisthaler, A.
Mikoviny, T.
Fuelberg, H. E.
Blake, D. R.
Huey, G.
Weinheimer, A. J.
Knapp, D. J.
Brune, W. H.
TI Emissions of black carbon, organic, and inorganic aerosols from biomass
burning in North America and Asia in 2008
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TRANSFORM INFRARED-SPECTROSCOPY; IONIZATION MASS-SPECTROMETRY;
LASER-INDUCED INCANDESCENCE; CENTRAL MEXICAN PLATEAU; LIGHT-ABSORPTION;
TRACE GASES; AIRCRAFT MEASUREMENTS; GLOBAL PRECIPITATION;
PHYSICAL-PROPERTIES; FIRE EMISSIONS
AB Reliable assessment of the impact of aerosols emitted from boreal forest fires on the Arctic climate necessitates improved understanding of emissions and the microphysical properties of carbonaceous (black carbon (BC) and organic aerosols (OA)) and inorganic aerosols. The size distributions of BC were measured by an SP2 based on the laser-induced incandescence technique on board the DC-8 aircraft during the NASA ARCTAS campaign. Aircraft sampling was made in fresh plumes strongly impacted by wildfires in North America (Canada and California) in summer 2008 and in those transported from Asia (Siberia in Russia and Kazakhstan) in spring 2008. We extracted biomass burning plumes using particle and tracer (CO, CH3CN, and CH2Cl2) data. OA constituted the dominant fraction of aerosols mass in the submicron range. The large majority of the emitted particles did not contain BC. We related the combustion phase of the fire as represented by the modified combustion efficiency (MCE) to the emission ratios between BC and other species. In particular, we derived the average emission ratios of BC/CO = 2.3 +/- 2.2 and 8.5 +/- 5.4 ng m(-3)/ppbv for BB in North America and Asia, respectively. The difference in the BC/CO emission ratios is likely due to the difference in MCE. The count median diameters and geometric standard deviations of the lognormal size distribution of BC in the BB plumes were 136-141 nm and 1.32-1.36, respectively, and depended little on MCE. These BC particles were thickly coated, with shell/core ratios of 1.3-1.6. These parameters can be used directly for improving model estimates of the impact of BB in the Arctic.
C1 [Kondo, Y.; Matsui, H.; Moteki, N.; Sahu, L.; Takegawa, N.; Kajino, M.] Univ Tokyo, Res Ctr Adv Sci & Technol, Meguro Ku, Tokyo 1538904, Japan.
[Vay, S.; Diskin, G. S.; Anderson, B.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Blake, D. R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA.
[Brune, W. H.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Cubison, M. J.; Jimenez, J. L.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Fuelberg, H. E.] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
[Huey, 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 80305 USA.
[Wisthaler, A.; Mikoviny, T.] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria.
[Zhao, Y.] Univ Calif Davis, Air Qual Res Ctr, Davis, CA 95616 USA.
[Cubison, M. J.; Jimenez, J. L.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
RP Kondo, Y (reprint author), Univ Tokyo, Res Ctr Adv Sci & Technol, Meguro Ku, 4-6-1 Komaba, Tokyo 1538904, Japan.
EM y.kondo@atmos.rcast.u-tokyo.ac.jp; matsui@atmos.rcast.u-tokyo.ac.jp;
moteki@atmos.rcast.u-tokyo.ac.jp; lokesh@prl.res.in;
takegawa@atmos.rcast.u-tokyo.ac.jp; kajino@mri-jma.go.jp;
yjzhao@ucdavis.edu; michael.cubison@colorado.edu;
jose.jimenez@colorado.edu; stephanie.a.vay@nasa.gov;
glenn.s.diskin@nasa.gov; b.e.anderson@larc.nasa.gov;
armin.wisthaler@uibk.ac.at; tomas.mikoviny@uibk.ac.at;
fuelberg@met.fsu.edu; drblake@uci.edu; greg.huey@eas.gatech.edu;
wein@ucar.edu; david@ucar.edu; brune@meteo.psu.edu
RI Jimenez, Jose/A-5294-2008; Kajino, Mizuo/B-5645-2012; Kondo,
Yutaka/D-1459-2012
OI Jimenez, Jose/0000-0001-6203-1847;
FU NASA [USP-SMD-08-009, NNX08D39G]; Ministry of Education, Culture,
Sports, Science, and Technology (MEXT); Japan Science and Technology
Agency (JST); Japanese Ministry of the Environment [B-083]
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. P.O.
Wennberg provided the SO2 data used for the present study. We
thank M. Osuka for his assistance with the field measurements. R.
Yokelson provided very useful comments on the manuscript. The
meteorological data were supplied by the European Centre for
Medium-Range Weather Forecasts (ECWMF). 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). Y.Z. was
supported in part by the NASA Tropospheric Chemistry Program
(USP-SMD-08-009). M.J.C. and J.L.J. acknowledge NASA grant NNX08D39G.
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.
NR 112
TC 69
Z9 69
U1 6
U2 55
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 APR 19
PY 2011
VL 116
AR D08204
DI 10.1029/2010JD015152
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 754KE
UT WOS:000289852700009
ER
PT J
AU Ajello, JM
Mangina, RS
Strickland, DJ
Dziczek, D
AF Ajello, Joseph M.
Mangina, Rao S.
Strickland, Douglas J.
Dziczek, Dariusz
TI Laboratory studies of UV emissions from proton impact on N-2: The
Lyman-Birge-Hopfield band system for aurora analysis
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LOW-ENERGY H; RESOLUTION ELECTRON-IMPACT; TRANSPORT-THEORETIC MODEL;
HYDROGEN ATOM AURORA; CROSS-SECTIONS; ALPHA EMISSION; DISSOCIATIVE
EXCITATION; STATISTICAL-MODEL; N=3 STATES; ULTRAVIOLET
AB We have measured the emission cross sections of the Lyman-Birge-Hopfield (LBH) a (1)Pi(g) - X (1)Sigma(+)(g) band system and several atomic nitrogen (N I) multiplets (1200, 1243, 1493 angstrom) by H+ (proton) impact on N-2 over an impact energy range of 1-7 keV. The peak proton-impact-induced emission cross section of the LBH band system (1260-2500 angstrom) was measured to be 5.05 +/- 1.52 x 10 (17) cm(2) at 7 keV. To the best of our knowledge, the present LBH emission cross sections are reported for the first time in the far ultraviolet (FUV) wavelength range of 1100-1600 angstrom. The proton energy range in this study, when coupled with previously published 10-100 keV proton excited emissions of N I multiplets, provides a wide energy range of emission cross sections for proton energy loss transport codes. This energy range includes the peak cross section and the energy range for Born scaling. The reported measurements lead to an important component of monoenergetic yields for proton FUV auroral emission. Such yields, based on emission cross sections and transport modeling, allowed for convenient comparison of emission efficiencies between proton and electron aurora. In addition, we have measured the H Ly alpha, LBH, and N I multiplet emission cross sections for H-2(+) and H-3(+) ion impact on N-2 at 5 keV and found that the magnitude of H Ly a emission cross section, sigma(em)(Ly alpha), follows in the order of impact ion mass H-3(+) > H-2(+) > H+.
C1 [Ajello, Joseph M.; Mangina, Rao S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Strickland, Douglas J.] Computat Phys Inc, Springfield, VA 22151 USA.
[Dziczek, Dariusz] Nicolaus Copernicus Univ, Inst Phys, PL-97100 Torun, Poland.
RP Ajello, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM joseph.m.ajello@jpl.nasa.gov
RI Dziczek, Dariusz/G-3620-2014
FU NASA; National Science Foundation Office [0850396]; Astronomy and
Physics Research and Analysis Program; Cassini Data Analysis Program;
Space Physics Program Offices
FX This work was performed at the Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), under a contract with the
National Aeronautics and Space Administration (NASA). We gratefully
acknowledge financial support through NASA's Geospace and Planetary
Atmospheres programs, the National Science Foundation Office under grant
0850396, the Astronomy and Physics Research and Analysis Program, the
Cassini Data Analysis Program and Space Physics Program Offices. We
thank Lars Wahlin for helping establish operation of the Colutron ion
source at JPL and Ronald Cummings for his technician support. We have
benefited from discussions with B. Van Zyl of the University of Denver.
NR 68
TC 6
Z9 6
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR 19
PY 2011
VL 116
AR A00K03
DI 10.1029/2010JA016103
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 754KX
UT WOS:000289854600005
ER
PT J
AU Ruzmaikin, A
Feynman, J
Stoev, SA
AF Ruzmaikin, A.
Feynman, J.
Stoev, S. A.
TI Distribution and clustering of fast coronal mass ejections
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ACTIVE REGIONS; ACCELERATION; PATTERNS
AB The purpose of this paper is to investigate the statistical properties of high-speed coronal mass ejections (fast CMEs), which play a major role in Space Weather. We study the cumulative distribution of the initial CME speeds applying a new, advanced statistical method based on the scaling properties of averages of maximal speeds selected in time intervals of fixed sizes. This method allows us for the first time to obtain a systematic statistical description of the fast CME speeds. Using this method, we identify a self-similar (power law) high-speed portion of the spectrum of the speed maxima in the range of speeds from about 700 km/s to 2000 km/s. This self-similar range of the speed distribution provides a meaningful definition of "the fast" CMEs and indicates that these CMEs are produced by a process that is the same across the range of scales. The investigation of the temporal behavior of the fast CME events indicates that the time intervals between fast CMEs are not independent, i.e., fast CMEs arrive in clusters. We characterize the fast CMEs clustering by the exponent theta called the extremal index, which is the inverse of the averaged number of CMEs per cluster. An independent correlation analysis of the tail of the CME distribution confirms and further quantifies the temporal dependence among the fast CME events. To illustrate the predictive capabilities of the method, we identify clusters in the time series of CMEs with speeds greater than 1000 km/s and calculate their statistical characteristics such as the size and duration of the clusters. The method used in this paper can be applied to many other extreme geophysical events.
C1 [Ruzmaikin, A.; Feynman, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stoev, S. A.] Univ Michigan, Dept Stat, Ann Arbor, MI 48109 USA.
RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alexander.ruzmaikin@jpl.nasa.gov; joan.feynman@jpl.nasa.gov;
sstoev@umich.edu
FU Jet Propulsion Laboratory of the California Institute of Technology
under National Aeronautics and Space Administration; NSF [DMS-0806094]
FX We are grateful to anonymous reviewers for 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. S. Stoev was partially supported
by the NSF grant DMS-0806094.
NR 25
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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 APR 19
PY 2011
VL 116
AR A04220
DI 10.1029/2010JA016247
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 754KX
UT WOS:000289854600009
ER
PT J
AU Nunes, DC
Smrekar, SE
Fisher, B
Plaut, JJ
Holt, JW
Head, JW
Kadish, SJ
Phillips, RJ
AF Nunes, Daniel Cahn
Smrekar, Suzanne E.
Fisher, Brian
Plaut, Jeffrey J.
Holt, John W.
Head, James W.
Kadish, Seth J.
Phillips, Roger J.
TI Shallow Radar (SHARAD), pedestal craters, and the lost Martian layers:
Initial assessments
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID SOUTH POLAR-REGION; MEDUSAE FOSSAE FORMATION; IMPACT CRATERS; WIND
EROSION; GROUND ICE; NORTHERN-HEMISPHERE; CLIMATE-CHANGE; MARS;
DEPOSITS; SURFACE
AB Since their discovery, Martian pedestal craters have been interpreted as remnants of layers that were once regionally extensive but have since been mostly removed. Pedestals span from subkilometer to hundreds of kilometers, but their thickness is less than similar to 500 m. Except for a small equatorial concentration in the Medusae Fossae Formation, the nearly exclusive occurrence of pedestal craters in the middle and high latitudes of Mars has led to the suspicion that the lost units bore a significant fraction of volatiles, such as water ice. Recent morphological characterizations of pedestal deposits have further supported this view. Here we employ radar soundings obtained by the Shallow Radar (SHARAD) to investigate the volumes of a subset of the pedestal population, in concert with high-resolution imagery to assist our interpretations. From the analysis of 97 pedestal craters we find that large pedestals (diameter > 30 km) are relatively transparent to radar in their majority, with SHARAD being able to detect the base of the pedestal deposits, and possess an average dielectric permittivity of 4 +/- 0.5. In one of the cases of large pedestals in Malea Planum, layering is detected both in SHARAD data and in high-resolution imagery of the pedestal margins. We find that clutter is a major issue in the analysis of radar soundings for smaller pedestals, and tentative detection of the basal reflection occurs in only a few of the cases examined. These detections yield a higher average permittivity of similar to 6. The permittivity value derived for the larger pedestals, for which a basal reflection is unambiguous, is higher than that of pure water ice but lower than that of most silicate materials. A mixture of ice and silicates or an ice-free porous silicate matrix can explain a permittivity of similar to 4, and radar alone cannot resolve this nonuniqueness. Data from the Compact Reconnaissance Imaging Spectrometer (CRISM) tentatively confirms a mafic component in at least one pedestal in Malea Planum. Interpretation of SHARAD results can support either a mixture of ice and silicates or a porous silicate. The former is compatible with a model where nonpolar ice is periodically deposited in the midlatitudes as a result of obliquity variations. The latter is compatible with ash deposits, at least in where pedestals appear in volcanic centers such as Malea Planum.
C1 [Nunes, Daniel Cahn; Smrekar, Suzanne E.; Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
[Fisher, Brian] Brown Univ, Div Engn, Providence, RI 02912 USA.
[Holt, John W.] Univ Texas Austin, Inst Geophys, Austin, TX 78758 USA.
[Head, James W.; Kadish, Seth J.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Phillips, Roger J.] SW Res Inst, Boulder, CO 80302 USA.
RP Nunes, DC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 183-301, Pasadena, CA 91101 USA.
EM Daniel.Nunes@jpl.nasa.gov
FU Caltech; Mars Reconnaissance Orbiter program office; National
Aeronautics and Space Administration
FX We would like to acknowledge Stefania Mattei and her team at the SHARAD
Operations Center for their continued dedication to provide the best
quality data set possible, grazie mille a voi. We would also like to
thank Eldar Noe Dobrea for discussions regarding CRISM data. Caltech's
Summer Undergraduate Research Fellowship supported B. Fisher and the
initial thrust of this work. D. Nunes would like to thank the support
from Caltech Postdoctoral Scholar Program and the Mars Reconnaissance
Orbiter program office. The authors would like to acknowledge reviews by
Nadine Barlow and James Skinner, which helped improve the quality of
this manuscript. 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 81
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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 APR 19
PY 2011
VL 116
AR E04006
DI 10.1029/2010JE003690
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 754JR
UT WOS:000289851400002
ER
PT J
AU Kurtz, NT
Markus, T
Farrell, SL
Worthen, DL
Boisvert, LN
AF Kurtz, N. T.
Markus, T.
Farrell, S. L.
Worthen, D. L.
Boisvert, L. N.
TI Observations of recent Arctic sea ice volume loss and its impact on
ocean-atmosphere energy exchange and ice production
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID MODEL; FLUX; AMPLIFICATION; THICKNESS; CLIMATE; BALANCE; SHEBA; SNOW
AB Using recently developed techniques we estimate snow and sea ice thickness distributions for the Arctic basin through the combination of freeboard data from the Ice, Cloud, and land Elevation Satellite (ICESat) and a snow depth model. These data are used with meteorological data and a thermodynamic sea ice model to calculate ocean-atmosphere heat exchange and ice volume production during the 2003-2008 fall and winter seasons. The calculated heat fluxes and ice growth rates are in agreement with previous observations over multiyear ice. In this study, we calculate heat fluxes and ice growth rates for the full distribution of ice thicknesses covering the Arctic basin and determine the impact of ice thickness change on the calculated values. Thinning of the sea ice is observed which greatly increases the 2005-2007 fall period ocean-atmosphere heat fluxes compared to those observed in 2003. Although there was also a decline in sea ice thickness for the winter periods, the winter time heat flux was found to be less impacted by the observed changes in ice thickness. A large increase in the net Arctic ocean-atmosphere heat output is also observed in the fall periods due to changes in the areal coverage of sea ice. The anomalously low sea ice coverage in 2007 led to a net ocean-atmosphere heat output approximately 3 times greater than was observed in previous years and suggests that sea ice losses are now playing a role in increasing surface air temperatures in the Arctic.
C1 [Kurtz, N. T.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Kurtz, N. T.; Markus, T.; Farrell, S. L.; Worthen, D. L.; Boisvert, L. N.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Farrell, S. L.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, Cooperat Inst Climate Studies, College Pk, MD 20742 USA.
[Worthen, D. L.] RS Informat Syst, Mclean, VA USA.
[Boisvert, L. N.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP Kurtz, NT (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
EM nathan.t.kurtz@nasa.gov
RI Farrell, Sinead/F-5586-2010; Markus, Thorsten/D-5365-2012
OI Farrell, Sinead/0000-0003-3222-2751;
FU National Science Foundation (NSF)
FX The authors would like to thank two anonymous reviewers for their
invaluable suggestions, which helped in improving the manuscript. The
ECMWF data for this study are from the Research Data Archive (RDA),
which is maintained by the Computational and Information Systems
Laboratory (CISL) at the National Center for Atmospheric Research
(NCAR). NCAR is sponsored by the National Science Foundation (NSF). The
original data are available from the RDA (http://dss.ucar.edu) in data
set number ds627.0. We also acknowledge NSIDC for providing the AMSR-E
and ICESat data used in this study (http://nsidc.org/).
NR 47
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SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR 16
PY 2011
VL 116
AR C04015
DI 10.1029/2010JC006235
PG 19
WC Oceanography
SC Oceanography
GA 751VY
UT WOS:000289647000001
ER
PT J
AU Ashley, JW
Golombek, MP
Christensen, PR
Squyres, SW
McCoy, TJ
Schroder, C
Fleischer, I
Johnson, JR
Herkenhoff, KE
Parker, TJ
AF Ashley, J. W.
Golombek, M. P.
Christensen, P. R.
Squyres, S. W.
McCoy, T. J.
Schroeder, C.
Fleischer, I.
Johnson, J. R.
Herkenhoff, K. E.
Parker, T. J.
TI Evidence for mechanical and chemical alteration of iron-nickel
meteorites on Mars: Process insights for Meridiani Planum
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ANTARCTIC METEORITES; ORDINARY CHONDRITES; CARBONACEOUS CHONDRITES;
GALACTIC EVOLUTION; BURNS FORMATION; GROUND ICE; ORIGIN; SURFACE;
OXIDATION; SILICON
AB The weathering of meteorites found on Mars involves chemical and physical processes that can provide clues to climate conditions at the location of their discovery. Beginning on sol 1961, the Opportunity rover encountered three large iron meteorites within a few hundred meters of each other. In order of discovery, these rocks have been assigned the unofficial names Block Island, Shelter Island, and Mackinac Island. Each rock presents a unique but complimentary set of features that increase our understanding of weathering processes at Meridiani Planum. Significant morphologic characteristics interpretable as weathering features include (1) a large pit in Block Island, lined with delicate iron protrusions suggestive of inclusion removal by corrosive interaction; (2) differentially eroded kamacite and taenite lamellae in Block Island and Shelter Island, providing relative timing through crosscutting relationships with deposition of (3) an iron oxide-rich dark coating; (4) regmaglypted surfaces testifying to regions of minimal surface modification, with other regions in the same meteorites exhibiting (5) large-scale, cavernous weathering (in Shelter Island and Mackinac Island). We conclude that the current size of the rocks is approximate to their original postfall contours. Their morphology thus likely results from a combination of atmospheric interaction and postfall weathering effects. Among our specific findings is evidence supporting (1) at least one possible episode of aqueous acidic exposure for Block Island; (2) ripple migration over portions of the meteorites; (3) a minimum of two separate episodes of wind abrasion; alternating with (4) at least one episode of coating-forming chemical alteration, most likely at subzero temperatures.
C1 [Ashley, J. W.; Christensen, P. R.] Arizona State Univ, Sch Earth & Space Explorat, Mars Space Flight Facil, Tempe, AZ 85287 USA.
[Golombek, M. P.; Parker, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[McCoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Schroeder, C.] Univ Tubingen, Ctr Appl Geosci, Tubingen, Germany.
[Fleischer, I.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Mainz, Germany.
[Johnson, J. R.; Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
RP Ashley, JW (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Mars Space Flight Facil, Tempe, AZ 85287 USA.
RI Schroder, Christian/B-3870-2009; Johnson, Jeffrey/F-3972-2015
OI Schroder, Christian/0000-0002-7935-6039;
FU NASA [NNX06-AD83H]
FX We would like to express our sincerest thanks to our two anonymous
reviewers. Jonathan Hill and Eliana McCartney were supportive in the
acquisition of data products. Marc Fries was helpful in preliminary
discussions. Ella Mae Lee and Bonnie Redding from the USGS team are
thanked for assembling the MI mosaics for this paper. Laurence Garvie of
Arizona State University's Center for Meteorite Studies is acknowledged
for access to meteorite collections and discussions. For the MIPL
geometric model of Block Island, we thank Nick Ruoff for tiepointing and
localization, Oleg Pariser for meshing, Kris Capraro for masking off bad
areas, Zareh Gorjian and Mike Stetson for cleaning up the model and
determining the volume, and Bob Deen for overseeing the effort. Funding
was provided in part through NASA Graduate Student Researchers Program
grant NNX06-AD83H.
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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 APR 16
PY 2011
VL 116
AR E00F20
DI 10.1029/2010JE003672
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 751WA
UT WOS:000289647200001
ER
PT J
AU Thaisen, KG
Head, JW
Taylor, LA
Kramer, GY
Isaacson, P
Nettles, J
Petro, N
Pieters, CM
AF Thaisen, Kevin G.
Head, James W.
Taylor, Lawrence A.
Kramer, Georgiana Y.
Isaacson, Peter
Nettles, Jeff
Petro, Noah
Pieters, Carle M.
TI Geology of the Moscoviense Basin
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID PEAK-RING FORMATION; MULTIRING BASINS; IMPACT CRATERS; LUNAR; MOON;
EVOLUTION; VOLCANISM; MISSION; SELENE; CHICXULUB
AB The Moscoviense Basin, on the northern portion of the lunar farside, displays topography with a partial peak ring, in addition to rings that are offset to the southeast. These rings do not follow the typical concentric ring spacing that is recognized with other basins, suggesting that they may have formed as a result of an oblique impact or perhaps multiple impacts. In addition to the unusual ring spacing present, the Moscoviense Basin contains diverse mare basalt units covering the basin floor and a few highland mafic exposures within its rings. New analysis of previously mapped mare units suggests that the oldest mare unit is the remnant of the impact melt sheet. The Moscoviense Basin provides a glimpse into the lunar highlands terrain and an opportunity to explore the geologic context of initial lunar crustal development and modification.
C1 [Thaisen, Kevin G.; Taylor, Lawrence A.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[Head, James W.; Isaacson, Peter; Nettles, Jeff; Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Kramer, Georgiana Y.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Petro, Noah] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kramer, Georgiana Y.] Lunar & Planetary Inst, Houston, TX 77058 USA.
RP Thaisen, KG (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, 1412 Circle Dr, Knoxville, TN 37996 USA.
EM kthaisen@utk.edu
RI Petro, Noah/F-5340-2013
FU NASA [NNM05AB26C]
FX M3 is supported as a NASA Discovery Program mission of
opportunity. The science results and science validation is supported
through NASA contract NNM05AB26C. The M3 team is honored to
have had the opportunity to fly as a guest instrument on Chandrayaan-1
and is grateful to all the ISRO team that enabled M3 data to
be returned. We gratefully acknowledge the valuable input to this
project by the public release of SELENE Terrain Camera data and LRO
Laser Altimeter data.
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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 APR 16
PY 2011
VL 116
AR E00G07
DI 10.1029/2010JE003732
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 751WA
UT WOS:000289647200002
ER
PT J
AU Grange, ML
Nemchin, AA
Timms, N
Pidgeon, RT
Meyer, C
AF Grange, M. L.
Nemchin, A. A.
Timms, N.
Pidgeon, R. T.
Meyer, C.
TI Complex magmatic and impact history prior to 4.1 Ga recorded in zircon
from Apollo 17 South Massif aphanitic breccia 73235
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID URANIUM-LEAD AGES; PLASTIC-DEFORMATION; MELT BRECCIAS; LUNAR; STATION-2;
BOULDER-1; MANTLE; CHEMISTRY; EVOLUTION; HIGHLANDS
AB Sample 73235 is one of several aphanitic impact melt breccias collected by the Apollo 17 mission at stations 2 and 3 on the slopes of the South Massif. This study presents a detailed investigation of internal structures and U-Pb ages of large zircon grains from this breccia sample. New data combined with the results of previous studies of zircon grains from the same location indicate that most zircon clasts in breccias from stations 2 and 3 formed during multiple magmatic events between 4.37 and 4.31 Ga, although the oldest zircon crystallized at about 4.42 Ga and the youngest at 4.21 Ga. In addition, zircons from the aphanitic breccias record several impact events prior to the similar to 3.9 Ga Late Heavy Bombardment. The results indicate that the zircons probably crystallized at different locations within the Procellarum KREEEP Terrane and were later excavated and modified by several impacts and delivered to the same locality within separate ejecta blankets. This locality became a source of material that formed the aphanitic impact melt breccias of the South Massif during a similar to 3.9 Ga impact. However, the zircons, showing old impact features, are not modified by this similar to 3.9 Ga impact event suggesting that (i) this common source area was located at the periphery of excavation cavity, and (ii) the > 3.9 Ga ages recorded by the zircon grains could date large (basin-forming) events as significant as major later (similar to 3.9 Ga) collisions such as Imbrium and Serenitatis. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Grange, M. L.; Nemchin, A. A.; Timms, N.; Pidgeon, R. T.] Curtin Univ, Western Australian Sch Mines, Dept Appl Geol, Perth, WA 6845, Australia.
[Nemchin, A. A.] Univ Munster, Inst Mineral, D-48149 Munster, Germany.
[Meyer, C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Grange, ML (reprint author), Curtin Univ, Western Australian Sch Mines, Dept Appl Geol, GPO Box U1987, Perth, WA 6845, Australia.
EM m.grange@curtin.edu.au
RI Grange, Marion/B-1449-2013;
OI Timms, Nicholas/0000-0003-2997-4303; Grange, Marion/0000-0001-6405-8795
FU Curtin Internal Research Grant; DFG
FX We want to thank the NASA, and especially the crew of Apollo 17 as none
of the samples will be available for the study without their hard work.
We are also grateful to Marc Norman, Liu Dunyi and Odette James for
their constructive comments that helped improve the paper. M. G. and
N.T. acknowledge funding from a Curtin Internal Research Grant. Rob Hart
is thanked for his assistance with scanning electron microscopy. A.N.
research at Munster University is currently supported by DFG.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 15
PY 2011
VL 75
IS 8
BP 2213
EP 2232
DI 10.1016/j.gca.2011.01.036
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 796EJ
UT WOS:000293033100014
ER
PT J
AU Danielson, S
Eisner, L
Weingartner, T
Aagaard, K
AF Danielson, S.
Eisner, L.
Weingartner, T.
Aagaard, K.
TI Thermal and haline variability over the central Bering Sea shelf:
Seasonal and interannual perspectives
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Bering Sea; Seasonal variability; Interannual variability; Temperature;
Salinity; Ekman transport
ID ALASKA COASTAL CURRENT; ARCTIC-OCEAN; ALEUTIAN LOW; FRESH-WATER; HEAT
FLUXES; ICE; CIRCULATION; ECOSYSTEM; PATTERNS; PACIFIC
AB We examine multi-year conductivity-temperature-depth (CTD) data to better understand temperature and salinity variability over the central Bering Sea shelf. Particular consideration is given to observations made annually from 2002 to 2007 between August and October, although other seasons and years are also considered. Vertical and horizontal correlation maps show that near-surface and near-bottom salinity anomalies tend to fluctuate in phase across the central shelf, but that temperature anomalies are vertically coherent only in the weakly or unstratified inner-shelf waters. We formulate heat content (HC) and freshwater content (FWC) budgets based on the CTD observations, direct estimates of external fluxes (surface heat fluxes, ice melt, precipitation (P), evaporation (E) and river discharge), and indirect estimates of advective contributions. Ice melt, P - E, river discharge, and along-isobath advection are sufficient to account for the mean spring-to-fall increase in FWC, while summer surface heat fluxes are primarily responsible for the mean seasonal increase in HC, although interannual variability in the HC at the end of summer appears related to variability in the along-isobath advection during the summer months. On the other hand, FWC anomalies at the end of summer are significantly correlated with the mean wind direction and cross-isobath Ekman transport averaged over the previous winter. Consistent with the latter finding, salinities exhibit a weak but significant inverse correlation between the coastal and mid-shelf waters. The cross-shelf transport likely has significant effect on nutrient fluxes and other processes important to the functioning of the shelf ecosystem. Both the summer and winter advection fields appear to result from the seasonal mean position and strength of the Aleutian Low. We find that interannual thermal and haline variability over the central Bering Sea shelf are largely uncoupled. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Danielson, S.; Weingartner, T.] Univ Alaska Fairbanks, Inst Marine Sci, Sch Fisheries & Ocean Sci, Fairbanks, AK 99775 USA.
[Eisner, L.] Natl Marine Fisheries Serv, NOAA, Alaska Fisheries Sci Ctr, Ted Stevens Marine Res Inst, Juneau, AK USA.
[Aagaard, K.] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
RP Danielson, S (reprint author), Univ Alaska Fairbanks, Inst Marine Sci, Sch Fisheries & Ocean Sci, Rm 114,ONeill Bldg, Fairbanks, AK 99775 USA.
EM seth@ims.uaf.edu
FU BASIS scientists at NOAA/AFSC; NOAA/PMEL; NSF [HLY-07-01, HLY-08-03,
KN195-10, ARC-0732428, ARC-0732771]; Arctic-Yukon-Kuskokwim Sustainable
Salmon Initiative; Bering Sea Fisherman's Association; NOAA; National
Marine Fisheries Service; North Pacific Research Board [NPMRI 12130];
Arctic Yukon Kuskokwim Sustainable Salmon Initiative [1195952]
FX This manuscript would not have been possible without the
cross-institutional and cross-disciplinary collaboration that has been
fostered through the BASIS and BEST programs. We particularly thank Ed
Farley and the rest of the BASIS scientists at NOAA/AFSC for their
support. Many thanks to Kristin Cieciel for survey logistics,
oceanographic data collection, CTD data processing, and database
maintenance; John Pohl and Alex Andrews for oceanographic data
collection; Jennifer Lanksbury for database design and maintenance; Rolf
Gradinger, Katrin Iken, and Bodil Bluhm for sharing their ice station
data; and Phyllis Stabeno for sharing M2 mooring data and BEST CTD data,
both collected with the support of the NOAA/PMEL Eco-FOCI program. We
thank he dedicated crews of the F/V Sea Storm, F/V NW Explorer, R/V
Oscar Dyson, R/V Knorr, R/V Point Sur, and the USCGC Healy for the many
successful BASIS and BEST cruises. We thank the BEST program scientists
and field crews for the LID data collections and processing. Data from
NSF sponsored BEST cruises HLY-07-01, HLY-08-03, and KN195-10 were taken
under the direction of chief scientist R. Sambrotto, Lamont-Doherty
Earth Observatory, Palisades, NY; data from cruise HLY-08-02 were taken
under the direction of chief scientist Carin Ashjian, Woods Hole
Oceanographic Institute, Woods Hole, MA; and data from cruise HLY-09-01
were taken under the direction of chief scientist Lee Cooper, University
of Maryland Center for Environmental Science, Solomons, MD. The
manuscript was improved with valuable comments from two anonymous
reviewers. BASIS oceanographic data collection was funded by the
Arctic-Yukon-Kuskokwim Sustainable Salmon Initiative, the Bering Sea
Fisherman's Association, NOAA Fisheries and the Environment (FATE)
program, and the National Marine Fisheries Service. Drifter data were
collected under funding from the North Pacific Research Board, Grant
NPMRI 12130, and the Arctic Yukon Kuskokwim Sustainable Salmon
Initiative, Grant ADN #1195952. This manuscript is listed as BEST/BSIERP
Publication #6. K. Aagaard was supported by NSF Grant ARC-0732428. S.
Danielson and T. Weingartner received financial support from the Bering
Sea Fisherman's Association Grant AC-299 and NSF Grant ARC-0732771.
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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 APR 15
PY 2011
VL 31
IS 6
BP 539
EP 554
DI 10.1016/j.csr.2010.12.010
PG 16
WC Oceanography
SC Oceanography
GA 765ZE
UT WOS:000290747100003
ER
PT J
AU Righter, K
King, C
Danielson, L
Pando, K
Lee, CT
AF Righter, K.
King, C.
Danielson, L.
Pando, K.
Lee, C. T.
TI Experimental determination of the metal/silicate partition coefficient
of Germanium: Implications for core and mantle differentiation
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Germanium; Core formation; Siderophile; Mantle; Differentiation
ID SILICATE MELT COMPOSITION; SIDEROPHILE ELEMENTS; IRON-METEORITES;
HIGH-PRESSURE; MAGMA OCEAN; ISOTOPIC VARIATIONS; BASALTIC GLASSES;
HIGH-TEMPERATURE; OXYGEN FUGACITY; TRACE-ELEMENTS
AB Germanium is a moderately siderophile, and volatile element that exhibits a depletion in Earth's mantle and other planetary and asteroidal basalts (relative to chondritic values). Attempts to explain these depletions have not been satisfactory, but there have also been too few experimental studies to constrain the chemical behavior of Ge. Experimental data have been challenging due to difficulties in analyzing the low (1 to 100 ppm) concentrations of Ge in silicate melts. In this study we examine the role of temperature and silicate melt composition in controlling the value of D(Ge) metal/silicate, by carrying out new experiments at high temperature and pressure. The experimental glasses were analyzed using laser-ablation ICP-MS, which can detect levels of Ge much lower than possible with the electron microprobe. Our new results show that D(Ge) metal/silicate decreases with increasing temperature over the range from 1500 to 1900 degrees C. Additionally, changing silicate melt composition from basalt to peridotite causes a small increase in D(Ge) metal/silicate, compared to the decrease observed in previous studies across a different range of melt composition. These results, combined with previous studies at higher pressures and with S-bearing metallic liquids, show that there are high PT conditions at which the Ge concentration Earth's primitive upper mantle can be explained through metal-silicate equilibrium in a magma ocean stage, where equilibration took place at 40 (+/- 4) GPa and 3200 (+/- 200) degrees C. Additionally, estimated Ge contents of the lunar, Martian and HED parent body mantles can be explained by magma ocean conditions in all of these bodies early in the solar system. These calculations all take into account both the volatile and siderophile nature of Ge. Published by Elsevier B.V.
C1 [Righter, K.; Danielson, L.; Pando, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[King, C.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[King, C.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Lee, C. T.] Rice Univ, Dept Earth Sci, Houston, TX 77005 USA.
RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
RI Lee, Cin-Ty/A-5469-2008
FU Lunar and Planetary Institute (LPI); RTOP; Packard Fellowship
FX C. King was supported by a summer internship at the Lunar and Planetary
Institute (LPI). The research was supported by an RTOP to K. Righter and
a Packard Fellowship to C.-T. Lee. V. LeRoux provided assistance with
the LA-ICP-MS analysis, as did A. Peslier and L Le on the electron
microprobe at JSC. The manuscript benefitted from the journal reviews of
D. Walker and an anonymous reviewer.
NR 77
TC 16
Z9 16
U1 2
U2 19
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 APR 15
PY 2011
VL 304
IS 3-4
BP 379
EP 388
DI 10.1016/j.epsl.2011.02.015
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 767EV
UT WOS:000290839000009
ER
PT J
AU Simon, JI
Young, ED
AF Simon, Justin I.
Young, Edward D.
TI Resetting, errorchrons and the meaning of canonical CAI initial
Al-26/Al-27 values
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE solar nebula; chronology; 26Al; open system resetting; isochrons; CAIs
ID AL-RICH INCLUSIONS; EARLY SOLAR-SYSTEM; MAGNESIUM ISOTOPE HETEROGENEITY;
REFRACTORY INCLUSIONS; SELF-DIFFUSION; ALLENDE; NEBULA; MG;
FRACTIONATION; EVAPORATION
AB The difference between the precise MC-ICPMS analyses of bulk calcium-aluminum-rich inclusion (CAI) fragments (e.g., Jacobsen et al., 2008) and supra-canonical values obtained by micro-analytical techniques, e.g., laser ablation MC-ICPMS (Young et al., 2005) and SIMS (Taylor et al., 2005), at face value seems to be problematic and therefore leads many to dismiss claims of the solar system (Al-26/Al-22)(o) greater than similar to 5 x 10(-5) as spurious. Here we use mass balance calculations to quantify the importance of open system isotopic exchange during CAI evolution and show that in situ supra-canonical, in-situ canonical, and bulk canonical measurements can all exist for an individual CAI. The calculations describe mechanisms of isotopic exchange that may have occurred early (100's ka) and late (similar to 1.5 Ma) in the solar nebula and much later (> 10's Ma) on parent body planetesimals. A range of possible modal mineralogies is modeled in order to populate the compositional space defined by in situ and bulk CAI measurements. In support of these simulated data we. describe in situ measurements of Al-27/Mg-24, Mg-25/Mg-24, and Mg-26/Mg-24 obtained by IA-MC-ICPMS comprising core-to-rim traverses across three CV3 CAls. The CAls exhibit distinctive Mg isotopic zoning profiles and varying abundances of daughter products of the short-lived nuclide Al-26 that are consistent with varying amounts of open system isotope exchange. Published by Elsevier B.V.
C1 [Simon, Justin I.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off KR111, Houston, TX 77058 USA.
[Young, Edward D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Young, Edward D.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
RP Simon, JI (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res Off KR111, Houston, TX 77058 USA.
EM Justin.I.Simon@NASA.gov
RI Simon, Justin/D-7015-2011
FU NASA; NASA Astrobiology Institute; National Science Foundation (USA);
NASA Johnson Space Cente
FX Discussions with K. McKeegan, A. Davis, M. Ito, Q. Yin, B. Jacobsen, S.
Jacobsen, I. Hutcheon, A. Galy, and O. Lovera are greatly appreciated.
As are input and sample material provided by S. Russell. Critical and
helpful reviews by A. Davis and T. Fagan improve the clarity of the
manuscript. This work was supported by grants from the NASA
Cosmochemistry program, the NASA Astrobiology Institute, and the
National Science Foundation (USA). J. Simon acknowledges support from
NASA Johnson Space Center and wishes to thank D. DePaolo and P. Renne
for their support of his postdoctoral research over which time some of
the ideas and calculations for this contribution originated.
NR 60
TC 8
Z9 8
U1 1
U2 6
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 APR 15
PY 2011
VL 304
IS 3-4
BP 468
EP 482
DI 10.1016/j.epsl.2011.02.023
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 767EV
UT WOS:000290839000017
ER
PT J
AU Sakamoto, T
Barbier, L
Barthelmy, SD
Cummings, JR
Fenimore, EE
Gehrels, N
Krimm, HA
Markwardt, CB
Palmer, DM
Parsons, AM
Sato, G
Stamatikos, M
Tueller, J
AF Sakamoto, T.
Barbier, L.
Barthelmy, S. D.
Cummings, J. R.
Fenimore, E. E.
Gehrels, N.
Krimm, H. A.
Markwardt, C. B.
Palmer, D. M.
Parsons, A. M.
Sato, G.
Stamatikos, M.
Tueller, J.
TI Probing the nature of short swift bursts via deep INTEGRAL monitoring of
GRB 050925
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Gamma-ray; Burst
ID GAMMA-RAY BURSTS; SGR-1900+14; SGR-1806-20; DISCOVERY; EMISSION; HETE-2;
FLARE
AB We present results from Swift, XMM-Newton, and deep INTEGRAL monitoring in the region of GRB 050925. This short Swift burst is a candidate for a newly discovered soft gamma-ray repeater (SGR) with the following observational burst properties: (1) galactic plane (b = -0.1 degrees) localization, (2) 150 ms duration, and (3) a blackbody rather than a simple power-law spectral shape (with a significance level of 97%). We found two possible X-ray counterparts of GRB 050925 by comparing the X-ray images from Swift XRT and XMM-Newton. Both X-ray sources show the transient behavior with a power-law decay index shallower than -1. We found no hard X-ray emission nor any additional burst from the location of GRB 050925 in similar to 5 ms of INTEGRAL data. We discuss about the three BATSE short bursts which might be associated with GRB 050925, based on their location and the duration. Assuming GRB 050925 is associated with the H-11 regions (W 58) at the galactic longitude of l = 70 degrees, we also discuss the source frame properties of GRB 050925. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Sakamoto, T.; Cummings, J. R.; Krimm, H. A.; Markwardt, C. B.] CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, T.; Barbier, L.; Barthelmy, S. D.; Cummings, J. R.; Gehrels, N.; Krimm, H. A.; Markwardt, C. B.; Parsons, A. M.; Tueller, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sakamoto, T.; Cummings, J. R.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Fenimore, E. E.; Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Sato, G.] JAXA, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan.
[Stamatikos, M.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
RP Sakamoto, T (reprint author), CRESST, Greenbelt, MD 20771 USA.
EM Taka.Sakamoto@nasa.gov
RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller,
Jack/D-5334-2012; Parsons, Ann/I-6604-2012
NR 23
TC 3
Z9 3
U1 0
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2011
VL 47
IS 8
BP 1346
EP 1352
DI 10.1016/j.asr.2010.08.004
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 758CE
UT WOS:000290136700011
ER
PT J
AU Stratta, G
Pozanenko, A
Atteia, JL
Klotz, A
Basa, S
Gendre, B
Verrecchia, F
Boer, M
Cutini, S
Henze, M
Holland, S
Ibrahimov, M
Ienna, F
Khamitov, I
Klose, S
Rumyantsev, V
Biryukov, V
Vachier, F
Arnouts, S
Perley, D
AF Stratta, G.
Pozanenko, A.
Atteia, J. L.
Klotz, A.
Basa, S.
Gendre, B.
Verrecchia, F.
Boer, M.
Cutini, S.
Henze, M.
Holland, S.
Ibrahimov, M.
Ienna, F.
Khamitov, I.
Klose, S.
Rumyantsev, V.
Biryukov, V.
Vachier, F.
Arnouts, S.
Perley, D.
TI The origin of the prompt optical emission in GRB 060111B
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Gamma-ray burst; Non-thermal radiation
ID GAMMA-RAY BURSTS
AB The detection of a bright optical emission measured with good temporal resolution during the prompt phase makes ORB 060111B a rare event that is especially useful for constraining theories of the prompt optical emission. Comparing this burst with other GRBs with evidence of optical peaks, we find that the optical peak epoch (t(p)) is anti-correlated with the high energy burst energetic assuming an isotropic energy release (E-iso) in agreement with Liang et al. (2009), and that the steeper is the post-peak afterglow decay, the less is the agreement with the correlation. GRB 060111B is among the tatters and it does not match the correlation. The Cannonball scenario is also discussed and we find that this model cannot be excluded for GRB 060111B. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Stratta, G.; Gendre, B.; Verrecchia, F.; Cutini, S.] ASI Sci Data Ctr, ASDC, I-00044 Frascati, Italy.
[Pozanenko, A.] Space Res Inst IKI, Moscow 117997, Russia.
[Atteia, J. L.; Ienna, F.] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France.
[Klotz, A.] Univ Toulouse, CESR, CNRS, UMR 5187, F-31028 Toulouse, France.
[Basa, S.] LAM OAM, F-13388 Marseille, France.
[Boer, M.] Observ Haute Provence, OHP, F-04870 St Michel Lobservatoire, France.
[Henze, M.; Klose, S.] Thueringer Landessternwarte, D-07778 Tautenburg, Germany.
[Holland, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ibrahimov, M.] Ulugh Beg Astron Inst, Tashkent 100052, Uzbekistan.
[Khamitov, I.] Akdeniz Univ Yerleskesi, TUBITAK Natl Observ, TR-07058 Antalya, Turkey.
[Rumyantsev, V.] SRI Crimean Astrophys Observ, Sci Res Inst, UA-98409 Nauchnyi, Crimea, Ukraine.
[Biryukov, V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Crimean Lab, UA-98409 Nauchnyi, Crimea, Ukraine.
[Vachier, F.] Observ Paris, IMCCE, F-92190 Paris, France.
[Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Perley, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Stratta, G (reprint author), ASI Sci Data Ctr, ASDC, Via Galileo Galilei, I-00044 Frascati, Italy.
EM stratta@asdc.asi.it
RI gendre, bruce/O-2923-2013; Stratta, Maria Giuliana/L-3045-2016;
OI gendre, bruce/0000-0002-9077-2025; Stratta, Maria
Giuliana/0000-0003-1055-7980; Verrecchia, Francesco/0000-0003-3455-5082;
Rumyantsev, Vasilij/0000-0003-1894-7019; Cutini,
Sara/0000-0002-1271-2924; Henze, Martin/0000-0001-9985-3406
NR 9
TC 1
Z9 1
U1 0
U2 4
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2011
VL 47
IS 8
BP 1413
EP 1415
DI 10.1016/j.asr.2010.06.014
PG 3
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 758CE
UT WOS:000290136700020
ER
PT J
AU Nishikawa, KI
Niemiec, J
Medvedev, M
Zhang, B
Hardee, P
Nordlund, A
Frederiksen, J
Mizuno, Y
Sol, H
Pohl, M
Hartmann, DH
Oka, M
Fishman, GJ
AF Nishikawa, K. -I.
Niemiec, J.
Medvedev, M.
Zhang, B.
Hardee, P.
Nordlund, A.
Frederiksen, J.
Mizuno, Y.
Sol, H.
Pohl, M.
Hartmann, D. H.
Oka, M.
Fishman, G. J.
TI Radiation from relativistic shocks in turbulent magnetic fields
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Acceleration of particles; Radiation; Jets; Gamma rays bursts; Magnetic
fields; Plasmas
ID GAMMA-RAY BURSTS; PARTICLE-ACCELERATION; COLLISIONLESS SHOCKS; WEIBEL
INSTABILITY; PROMPT EMISSION; FIREBALL MODEL; AFTERGLOWS; SIMULATIONS;
GENERATION; EVOLUTION
AB Using our new 3-D relativistic particle-in-cell (PIC) code parallelized with MPI, we investigated long-term particle acceleration associated with a relativistic electron positron jet propagating in an unmagnetized ambient electron positron plasma. The simulations were performed using a much longer simulation system than our previous simulations in order to investigate the full nonlinear stage of the Weibel instability and its particle acceleration mechanism. Cold jet electrons are thermalized and ambient electrons are accelerated in the resulting shocks. Acceleration of ambient electrons leads to a maximum ambient electron density three times larger than the original value as predicted by hydrodynamic shock compression. In the jet (reverse) shock behind the bow (forward) shock the strongest electromagnetic fields are generated. These fields may lead to time dependent afterglow emission. In order to calculate radiation from first principles that goes beyond the standard synchrotron model used in astrophysical objects we have used PIC simulations. Initially we calculated radiation from electrons propagating in a uniform parallel magnetic field to verify the technique. We then used the technique to calculate emission from electrons in a small simulation system. From these simulations we obtained spectra which are consistent with those generated from electrons propagating in turbulent magnetic fields with red noise. This turbulent magnetic field is similar to the magnetic field generated at an early nonlinear stage of the Weibel instability. A fully developed shock within a larger simulation system may generate a jitter/synchrotron spectrum. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Nishikawa, K. -I.; Mizuno, Y.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Niemiec, J.] Inst Nucl Phys PAN, PL-31342 Krakow, Poland.
[Medvedev, M.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA.
[Hardee, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Nordlund, A.; Frederiksen, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Sol, H.] Observ Paris, LUTH, F-92195 Meudon, France.
[Pohl, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Oka, M.] Univ Calif Berkeley, ISpace Sci Lab, Berkeley, CA 94720 USA.
[Fishman, G. J.] NASA MSFC, Huntsville, AL 35805 USA.
RP Nishikawa, KI (reprint author), Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
EM ken-ichi.nishikawa-l@nasa.gov
RI Nordlund, Aake/M-4528-2014; Frederiksen, Jacob Trier/P-6757-2015;
Mizuno, Yosuke/D-5656-2017
OI Nordlund, Aake/0000-0002-2219-0541; Frederiksen, Jacob
Trier/0000-0002-3560-0044; Mizuno, Yosuke/0000-0002-8131-6730
FU MNiSW [1 P03D 003 29, N N203 393034]; Foundation for Polish Science; EEA
Financial Mechanism; National Science Foundation NSF [PHY05-51164];
Danish Natural Science Research Council; [NSF-AST-0506719];
[AST-0506666]; [AST-0908040]; [AST-0908010]; [NASA-NNG05G-K73G];
[NNX07AJ88G]; [NNX08AG83G]; [NNX 08AL39G]; [NNX09AD16G]
FX This work is supported by NSF-AST-0506719, AST-0506666, AST-0908040,
AST-0908010, NASA-NNG05G-K73G, NNX07AJ88G, NNX08AG83G, NNX 08AL39G, and
NNX09AD16G. JN was supported by MNiSW research projects 1 P03D 003 29
and N N203 393034, and The Foundation for Polish Science through the
HOMING program, which is supported through the EEA Financial Mechanism.
Simulations were performed at the Columbia facility at the NASA Advanced
Supercomputing (NAS) and IBM p690 (Copper) at the National Center for
Supercomputing Applications (NCSA) which is supported by the NSF. Part
of this work was done while K.-I. N. was visiting the Niels Bohr
Institute. Support from the Danish Natural Science Research Council is
gratefully acknowledged. This report was finalized during the program
"Particle Acceleration in Astrophysical Plasmas" at the Kavli Institute
for Theoretical Physics which is supported by the National Science
Foundation under Grant No. PHY05-51164.
NR 48
TC 16
Z9 16
U1 0
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2011
VL 47
IS 8
BP 1434
EP 1440
DI 10.1016/j.asr.2011.01.032
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 758CE
UT WOS:000290136700024
ER
PT J
AU Sakamoto, T
Wallace, CA
Donato, D
Gehrels, N
Okajima, T
Ukwatta, TN
AF Sakamoto, T.
Wallace, C. A.
Donato, D.
Gehrels, N.
Okajima, T.
Ukwatta, T. N.
TI Goddard Robotic Telescope - Optical follow-up of GRBs and coordinated
observations of AGNs
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Gamma ray; Burst; AGN; Optical
ID GAMMA-RAY BURSTS; PROMPT; NUCLEI
AB Since it is not possible to predict when a Gamma-Ray Burst (GRB) will occur or when Active Galactic Nucleus (AGN) flaring activity starts, follow-up/monitoring ground telescopes must be located as uniformly as possible all over the world in order to collect data simultaneously with Fermi and Swift detections. However, there is a distinct gap in follow-up coverage of telescopes in the eastern U.S. region based on the operations of Swift. Motivated by this fact, we have constructed a 14 '' fully automated optical robotic telescope, Goddard Robotic Telescope (GRT), at the Goddard Geophysical and Astronomical Observatory. The aims of our robotic telescope are (1) to follow-up Swift/Fermi GRBs and (2) to perform the coordinated optical observations of Fermi Large Area Telescope (LAT) AGN. Our telescope system consists of off-the-shelf hardware. With the focal reducer, we are able to match the field of view of Swift narrow instruments (20' x 20'). We started scientific observations in mid-November 2008 and GRT has been fully remotely operated since August 2009. The 3 sigma upper limit in a 30s exposure in the R filter is similar to 15.4 mag; however, we can reach to similar to 18 mag in a 600 s exposures. Due to the weather condition at the telescope site, our observing efficiency is 30-40% on average. (c) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Sakamoto, T.; Donato, D.] CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, T.; Donato, D.; Gehrels, N.; Okajima, T.; Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sakamoto, T.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Wallace, C. A.] Florida Gulf Coast Univ, Ft Myers, FL 33965 USA.
[Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Okajima, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ukwatta, T. N.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
RP Sakamoto, T (reprint author), CRESST, Greenbelt, MD 20771 USA.
EM Taka.Sakamoto@nasa.gov
RI Gehrels, Neil/D-2971-2012
NR 11
TC 1
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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 APR 15
PY 2011
VL 47
IS 8
BP 1444
EP 1450
DI 10.1016/j.asr.2010.10.018
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 758CE
UT WOS:000290136700026
ER
PT J
AU Mawet, D
Serabyn, E
Wallace, JK
Pueyo, L
AF Mawet, Dimitri
Serabyn, Eugene
Wallace, J. Kent
Pueyo, Laurent
TI Improved high-contrast imaging with on-axis telescopes using a
multistage vortex coronagraph
SO OPTICS LETTERS
LA English
DT Article
AB The vortex coronagraph is one of the most promising coronagraphs for high-contrast imaging because of its simplicity, small inner working angle, high throughput, and clear off-axis discovery space. However, as with most coronagraphs, centrally obscured on-axis telescopes degrade contrast. Based on the remarkable ability of vortex coronagraphs to move light between the interior and exterior of pupils, we propose a method based on multiple vortices, that without sacrificing throughput, reduces the residual light leakage to (a/A)(n), with n >= 4, and a and A being the radii of the central obscuration and primary mirror, respectively. This method thus enables high contrasts to be reached even with an on-axis telescope. (c) 2011 Optical Society of America
C1 [Mawet, Dimitri; Serabyn, Eugene; Wallace, J. Kent; Pueyo, Laurent] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pueyo, Laurent] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Pueyo, Laurent] Johns Hopkins Univ, Baltimore, MD 21218 USA.
RP Mawet, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dmawet@eso.org
FU National Aeronautics and Space Administration; Carl Sagan Fellowship
Program
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. L. Pueyo acknowledge support from the Carl
Sagan Fellowship Program.
NR 11
TC 36
Z9 37
U1 0
U2 4
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 APR 15
PY 2011
VL 36
IS 8
BP 1506
EP 1508
PG 3
WC Optics
SC Optics
GA 756SH
UT WOS:000290034500067
PM 21499405
ER
PT J
AU Volz, MP
Mazuruk, K
AF Volz, M. P.
Mazuruk, K.
TI Existence and shapes of menisci in detached Bridgman growth
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE Bridgman technique; Detached growth; Microgravity conditions; Growth
from melt; Semiconducting germanium
ID GERMANIUM SINGLE-CRYSTALS; CRUCIBLE CONTACT; SOLIDIFICATION; MELTS;
MICROGRAVITY; DEPENDENCE; ANGLE
AB In detached Bridgman growth, the crystal radius is less than the crucible radius and a meniscus bridges the gap between the crystal and crucible wall. Existence of detached growth depends upon the contact angle of the melt with the crucible wall, the growth angle of the solidifying crystal, the pressure differential across the meniscus, and the Bond number. The Young-Laplace capillary equation is used to calculate the crystal radii of detached states as a function of the pressure differential across the meniscus. Both terrestrial and microgravity conditions are considered. A variety of solution states is found, and multiple solutions with different crystal radii can exist for a given value of the pressure differential. The meniscus shapes for the detached states vary from simply convex or concave to shapes with numerous inflections. An approximate solution to the Young-Laplace equation for small Bond numbers is derived. Published by Elsevier B.V.
C1 [Volz, M. P.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Mazuruk, K.] Univ Alabama, Huntsville, AL 35899 USA.
RP Volz, MP (reprint author), NASA, George C Marshall Space Flight Ctr, EM31, Huntsville, AL 35812 USA.
EM Martin.Volz@nasa.gov
FU NASA International Space Station
FX The authors gratefully acknowledge support from the NASA International
Space Station Research Project.
NR 27
TC 7
Z9 7
U1 2
U2 5
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 APR 15
PY 2011
VL 321
IS 1
BP 29
EP 35
DI 10.1016/j.jcrysgro.2011.02.035
PG 7
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA 757BC
UT WOS:000290057900006
ER
PT J
AU Schultz, JK
Becker, BL
Johanos, TC
Lopez, JU
Kashinsky, L
AF Schultz, Jennifer K.
Becker, Brenda L.
Johanos, Thea C.
Lopez, Jessica U.
Kashinsky, Lizabeth
TI Dizygotic twinning in the Hawaiian monk seal
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE fecundity; maternal investment; microsatellite; multiple maternity;
Monachus schauinslandi
ID ZEALAND FUR-SEAL; MONACHUS-SCHAUINSLANDI; FOSTERING BEHAVIOR;
REPRODUCTIVE-CYCLE; HALICHOERUS-GRYPUS; ELEPHANT SEALS; GREY SEALS;
SURVIVAL; PUP
AB Twinning is extremely rare in pinnipeds. Instances in which a female is observed simultaneously nursing 2 pups may represent alloparenting, or nonfilial nursing, a relatively common trait in pinnipeds. We explored the incidence of twinning in the Hawaiian monk seal (Monachus schauinslandi). We observed 7 sets of putative twins (i.e., an isolated female nursing 2 newborn pups) of 4,965 total births recorded between 1983 and 2008 (minimum twinning rate = 0.1%). Genetic specimens from the mother and both pups were available only for 5 of the 7 sets. Microsatellite genotyping revealed all of these to be dizygotic twins, with low probability of false assignment (P < 0.001). On average, Hawaiian monk seal twins were less likely to survive to weaning than singletons born in the same year and on the same island (P = 0.008). Those that weaned were smaller in size (i.e., axillary girths 1-4 SDs lower than singletons). In the critically endangered Hawaiian monk seal twinning appears to be a rare trait that results in overall lower survival rates but also offers a small opportunity for stock enhancement.
C1 [Schultz, Jennifer K.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA.
[Becker, Brenda L.; Johanos, Thea C.; Lopez, Jessica U.; Kashinsky, Lizabeth] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96814 USA.
RP Schultz, JK (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA.
EM jschultz@hawaii.edu
FU Marine Mammal Commission [GS00M04PDM0027]; Northwestern Hawaiian Islands
Coral Reef Ecosystem Reserve; Environmental Protection Agency STAR;
National Science Foundation [0549514]
FX We thank the numerous seasonal field crews for their efforts in the
collection of data, particularly S. Canja, S. Farry, J. Henderson, J.
Klavitter, L. Laniawe, R. Marshall, A. Dietrich, E. Green, J. Jones, J.
Palmer, and M. Vekasy. Drs. R. Braun and A. Aguirre conducted necropsies
on several of the dead twins. We thank F. Parrish, C. Littnan, J. Baker,
T. Wurth, and A. Harting for comments on the manuscript. For logistical
support we thank the Papahanaumokuakea Marine National Monument, United
States Fish and Wildlife Service, and the captain, officers, and crew of
the National Oceanic and Atmospheric Administration ships Townsend
Cromwell and Oscar Elton Sette. This research was performed under the
following National Marine Fisheries Service Scientific Research and
Enhancement permits: 413, 482, 489, 889, 848-1335, and 848-1695. Funding
was provided by the Marine Mammal Commission (research grant
GS00M04PDM0027) and the Northwestern Hawaiian Islands Coral Reef
Ecosystem Reserve. JKS was supported by Environmental Protection Agency
STAR and National Science Foundation IGERT fellowships (award 0549514;
principal investigator B. A. Wilcox). This is contribution 1416 from the
Hawai'i Institute of Marine Biology and contribution 8033 from the
School of Ocean and Earth Science and Technology at the University of
Hawai'i.
NR 36
TC 2
Z9 2
U1 0
U2 11
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-2372
EI 1545-1542
J9 J MAMMAL
JI J. Mammal.
PD APR 15
PY 2011
VL 92
IS 2
BP 336
EP 341
DI 10.1644/10-MAMM-A-275.1
PG 6
WC Zoology
SC Zoology
GA 754PV
UT WOS:000289869700008
ER
PT J
AU Masek, JG
Cohen, WB
Leckie, D
Wulder, MA
Vargas, R
de Jong, B
Healey, S
Law, B
Birdsey, R
Houghton, RA
Mildrexler, D
Goward, S
Smith, WB
AF Masek, Jeffrey G.
Cohen, Warren B.
Leckie, Donald
Wulder, Michael A.
Vargas, Rodrigo
de Jong, Ben
Healey, Sean
Law, Beverly
Birdsey, Richard
Houghton, R. A.
Mildrexler, David
Goward, Samuel
Smith, W. Brad
TI Recent rates of forest harvest and conversion in North America
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID LAND-USE CHANGE; REMOTELY-SENSED DATA; UNITED-STATES; CARBON STORAGE;
PONDEROSA PINE; WOOD PRODUCTS; COVER LOSS; MANAGEMENT-PRACTICES;
PACIFIC-NORTHWEST; TROPICAL FORESTS
AB Incorporating ecological disturbance into biogeochemical models is critical for estimating current and future carbon stocks and fluxes. In particular, anthropogenic disturbances, such as forest conversion and wood harvest, strongly affect forest carbon dynamics within North America. This paper summarizes recent (2000-2008) rates of extraction, including both conversion and harvest, derived from national forest inventories for North America (the United States, Canada, and Mexico). During the 2000s, 6.1 million ha/yr were affected by harvest, another 1.0 million ha/yr were converted to other land uses through gross deforestation, and 0.4 million ha/yr were degraded. Thus about 1.0% of North America's forests experienced some form of anthropogenic disturbance each year. However, due to harvest recovery, afforestation, and reforestation, the total forest area on the continent has been roughly stable during the decade. On average, about 110 m(3) of roundwood volume was extracted per hectare harvested across the continent. Patterns of extraction vary among the three countries, with U.S. and Canadian activity dominated by partial and clear-cut harvest, respectively, and activity in Mexico dominated by conversion (deforestation) for agriculture. Temporal trends in harvest and clearing may be affected by economic variables, technology, and forest policy decisions. While overall rates of extraction appear fairly stable in all three countries since the 1980s, harvest within the United States has shifted toward the southern United States and away from the Pacific Northwest.
C1 [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Birdsey, Richard] US Forest Serv, No Global Change Res Program, Newtown Sq, PA 19073 USA.
[Cohen, Warren B.] US Forest Serv, Pacific NW Res Stn, Corvallis, OR 97331 USA.
[de Jong, Ben] El Colegio Frontera Sur, Tabasco 86280, Mexico.
[Goward, Samuel] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Healey, Sean] US Forest Serv, Rocky Mt Res Stn, Ogden, UT 84401 USA.
[Houghton, R. A.] Woods Hole Res Ctr, Falmouth, MA 02543 USA.
[Law, Beverly] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Leckie, Donald; Wulder, Michael A.] Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC V8Z 1M5, Canada.
[Mildrexler, David] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
[Smith, W. Brad] US Forest Serv, Arlington, VA 22209 USA.
[Vargas, Rodrigo] Ctr Invest Cient & Educ Super Ensenada, Dept Biol Conservac, Ensenada 22830, Baja California, Mexico.
RP Masek, JG (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
EM jeffrey.g.masek@nasa.gov
RI Masek, Jeffrey/D-7673-2012; Trejo, Yesenia/D-9257-2012; Wulder,
Michael/J-5597-2016; Vargas, Rodrigo/C-4720-2008; Law,
Beverly/G-3882-2010
OI Wulder, Michael/0000-0002-6942-1896; Vargas,
Rodrigo/0000-0001-6829-5333; Law, Beverly/0000-0002-1605-1203
FU NASA; U.S. Forest Service; Canadian Forest Service; ECOSUR; Office of
Science (BER) U.S. Department of Energy [DE-FG02-04ER63911]
FX This work was prepared as part of the North American Carbon Program
(NACP) and CarbonNA activities, with support from the NASA Terrestrial
Ecology Program, the U.S. Forest Service, the Canadian Forest Service,
and ECOSUR. B.E.L. acknowledges the Office of Science (BER) U.S.
Department of Energy (award DE-FG02-04ER63911) for support of AmeriFlux
synthesis.
NR 120
TC 33
Z9 33
U1 2
U2 41
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD APR 15
PY 2011
VL 116
AR G00K03
DI 10.1029/2010JG001471
PG 22
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 751WL
UT WOS:000289648300002
ER
PT J
AU Goodrich, JP
Varner, RK
Frolking, S
Duncan, BN
Crill, PM
AF Goodrich, Jordan P.
Varner, Ruth K.
Frolking, Steve
Duncan, Bryan N.
Crill, Patrick M.
TI High-frequency measurements of methane ebullition over a growing season
at a temperate peatland site
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ART. NO. GB1003; ATMOSPHERIC METHANE; NATURAL WETLANDS; VASCULAR PLANTS;
WATER-TABLE; EXCHANGE; EMISSIONS; BIOGEOCHEMISTRY; DYNAMICS; CLIMATE
AB Bubbles can contribute a significant fraction of methane emissions from wetlands; however the range of reported fractions is very large and accurate characterization of this pathway has proven difficult. Here we show that continuous automated flux chambers combined with an integrated cavity output spectroscopy (ICOS) instrument allow us to quantify both CH4 ebullition rate and magnitude. For a temperate poor fen in 2009, ebullition rate varied on hourly to seasonal time scales. A diel pattern in ebullition was identified with peak release occurring between 20:00 and 06:00 local time, though steady fluxes (i.e., those with a linear increase in chamber headspace CH4 concentration) did not exhibit diel variability. Seasonal mean ebullition rates peaked at 843.5 +/- 384.2 events m(-2) d(-1) during the summer, with a mean magnitude of 0.19 mg CH4 released in each event. Citation: Goodrich, J. P., R. K. Varner, S. Frolking, B. N. Duncan, and P. M. Crill (2011), High-frequency measurements of methane ebullition over a growing season at a temperate peatland site, Geophys. Res. Lett., 38, L07404, doi: 10.1029/2011GL046915.
C1 [Goodrich, Jordan P.; Varner, Ruth K.; Frolking, Steve] Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03824 USA.
[Duncan, Bryan N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Crill, Patrick M.] Stockholm Univ, Dept Geol Sci, SE-10691 Stockholm, Sweden.
RP Goodrich, JP (reprint author), Univ New Hampshire, Complex Syst Res Ctr, 8 Coll Rd, Durham, NH 03824 USA.
EM jpd2@unh.edu
RI Varner, Ruth/E-5371-2011; Duncan, Bryan/A-5962-2011;
OI Varner, Ruth/0000-0002-3571-6629; Crill, Patrick/0000-0003-1110-3059
FU U.S. Department of Energy's Office of Science (BER) through the
Northeastern Regional Center of the National Institute for Climate
Change Research and the Research; University of New Hampshire; NASA GSFC
FX This research was supported in part by the U.S. Department of Energy's
Office of Science (BER) through the Northeastern Regional Center of the
National Institute for Climate Change Research and the Research and
Discover program by the University of New Hampshire and NASA GSFC.
Special thanks to Eduardo Miranda and Michael Keller for their
contributions to the success of this project.
NR 25
TC 22
Z9 22
U1 3
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 APR 15
PY 2011
VL 38
AR L07404
DI 10.1029/2011GL046915
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 751XA
UT WOS:000289649800003
ER
PT J
AU Vernier, JP
Thomason, LW
Kar, J
AF Vernier, J. -P.
Thomason, L. W.
Kar, J.
TI CALIPSO detection of an Asian tropopause aerosol layer
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID TIBETAN PLATEAU; STRATOSPHERIC AEROSOL; MONSOON ANTICYCLONE;
WATER-VAPOR; TROPOSPHERE; TRANSPORT; POLLUTION; SUMMER; SIMULATION;
EXCHANGE
AB The first four years of the CALIPSO lidar measurements have revealed the existence of an aerosol layer at the tropopause level associated with the Asian monsoon season in June, July and August. This Asian Tropopause Aerosol Layer (ATAL) extends geographically from Eastern Mediterranean (down to North Africa) to Western China (down to Thailand), and vertically from 13 to 18 km. The Scattering Ratio inferred from CALIPSO shows values between 1.10-1.15 on average with associated depolarization ratio of less than 5%. The Gaussian distribution of the points indicates that the mean value is statistically driven by an enhancement of the background aerosol level and not by episodic events such as a volcanic eruption or cloud contamination. Further satellite observations of aerosols and gases as well as field campaigns are urgently needed to characterize this layer, which is likely to be a significant source of non-volcanic aerosols for the global upper troposphere with a potential impact on its radiative and chemical balance. Citation: Vernier, J.-P., L. W. Thomason, and J. Kar (2011), CALIPSO detection of an Asian tropopause aerosol layer, Geophys. Res. Lett., 38, L07804, doi: 10.1029/2010GL046614.
C1 [Vernier, J. -P.; Thomason, L. W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Kar, J.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Vernier, JP (reprint author), NASA, Langley Res Ctr, Mail Stop 475, Hampton, VA 23681 USA.
EM jean-paul.vernier@nasa.gov
NR 30
TC 54
Z9 54
U1 5
U2 29
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 APR 15
PY 2011
VL 38
AR L07804
DI 10.1029/2010GL046614
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 751XA
UT WOS:000289649800001
ER
PT J
AU Jones, L
Dolinsky, V
Haykowsky, M
Patterson, I
Jones, L
Allen, J
Scott, J
Rogan, K
Khouri, M
Hornsby, W
Young, M
Peppercorn, J
Kimmick, G
Dyck, J
AF Jones, Lee
Dolinsky, Vernon
Haykowsky, Mark
Patterson, Ian
Jones, Lee
Allen, Jason
Scott, Jessica
Rogan, Kyle
Khouri, Michael
Hornsby, Whitney
Young, Martin
Peppercorn, Jeffrey
Kimmick, Gretchen
Dyck, Jason
TI Effects of aerobic training to improve cardiovascular function and
prevent cardiac remodeling after cytotoxic therapy in early breast
cancer
SO CANCER RESEARCH
LA English
DT Meeting Abstract
C1 [Jones, Lee; Jones, Lee; Allen, Jason; Khouri, Michael; Hornsby, Whitney; Peppercorn, Jeffrey; Kimmick, Gretchen] Duke Univ, Med Ctr, Durham, NC USA.
[Dolinsky, Vernon; Haykowsky, Mark; Patterson, Ian; Rogan, Kyle; Dyck, Jason] Univ Alberta, Edmonton, AB, Canada.
[Scott, Jessica] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Young, Martin] Univ Alabama Birmingham, Birmingham, AL USA.
NR 0
TC 2
Z9 2
U1 0
U2 0
PU AMER ASSOC CANCER RESEARCH
PI PHILADELPHIA
PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA
SN 0008-5472
EI 1538-7445
J9 CANCER RES
JI Cancer Res.
PD APR 15
PY 2011
VL 71
SU 8
MA 5024
DI 10.1158/1538-7445.AM2011-5024
PG 2
WC Oncology
SC Oncology
GA V43SO
UT WOS:000209701302473
ER
PT J
AU Wang, ML
Hada, M
Pluth, J
Anderson, J
O'Neill, P
Cucinotta, F
AF Wang, Minli
Hada, Megumi
Pluth, Janice
Anderson, Jennifer
O'Neill, Peter
Cucinotta, Francis
TI Ionizing radiation can enhance TGF beta induced EMT: Investigation of
signatures of cross-talk with the ATM pathway
SO CANCER RESEARCH
LA English
DT Meeting Abstract
C1 [Wang, Minli; Hada, Megumi] USRA NASA, Houston, TX USA.
[Pluth, Janice] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Anderson, Jennifer; O'Neill, Peter] Univ Oxford, Gray Inst Radiat Oncol & Biol, Oxford, England.
[Cucinotta, Francis] NASA Johnson Space Ctr, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER ASSOC CANCER RESEARCH
PI PHILADELPHIA
PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA
SN 0008-5472
EI 1538-7445
J9 CANCER RES
JI Cancer Res.
PD APR 15
PY 2011
VL 71
SU 8
MA LB-50
DI 10.1158/1538-7445.AM2011-LB-50
PG 2
WC Oncology
SC Oncology
GA V43SO
UT WOS:000209701303357
ER
PT J
AU Chen, J
Zhu, XL
Vogelmann, JE
Gao, F
Jin, SM
AF Chen, Jin
Zhu, Xiaolin
Vogelmann, James E.
Gao, Feng
Jin, Suming
TI A simple and effective method for filling gaps in Landsat ETM plus
SLC-off images
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat ETM; SLC-off; Gap filling
ID CONTERMINOUS UNITED-STATES; COVER; MODIS; CALIBRATION; SENSORS; TM
AB The scan-line corrector (SIC) of the Landsat 7 Enhanced Thematic Mapper Plus (ETM+) sensor failed in 2003, resulting in about 22% of the pixels per scene not being scanned. The SLC failure has seriously limited the scientific applications of ETM+ data. While there have been a number of methods developed to fill in the data gaps, each method has shortcomings, especially for heterogeneous landscapes. Based on the assumption that the same-class neighboring pixels around the un-scanned pixels have similar spectral characteristics, and that these neighboring and un-scanned pixels exhibit similar patterns of spectral differences between dates, we developed a simple and effective method to interpolate the values of the pixels within the gaps. We refer to this method as the Neighborhood Similar Pixel Interpolator (NSPI). Simulated and actual SIC-off ETM+ images were used to assess the performance of the NSPI. Results indicate that NSPI can restore the value of un-scanned pixels very accurately, and that it works especially well in heterogeneous regions. In addition, it can work well even if there is a relatively long time interval or significant spectral changes between the input and target image. The filled images appear reasonably spatially continuous without obvious striping patterns. Supervised classification using the maximum likelihood algorithm was done on both gap-filled simulated SIC-off data and the original "gap free" data set, and it was found that classification results, including accuracies, were very comparable. This indicates that gap-filled products generated by NSPI will have relevance to the user community for various land cover applications. In addition, the simple principle and high computational efficiency of NSPI will enable processing large volumes of SIC-off ETM+ data. Published by Elsevier Inc.
C1 [Vogelmann, James E.; Jin, Suming] USGS Earth Resources Observat & Sci EROS Ctr, ASRC Res & Technol Solut ARTS, Sioux Falls, SD 57198 USA.
[Chen, Jin; Zhu, Xiaolin] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China.
[Zhu, Xiaolin] Ohio State Univ, Dept Geog, Columbus, OH 43210 USA.
[Gao, Feng] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Gao, Feng] Earth Resources Technol Inc, Laurel, MD 20707 USA.
RP Vogelmann, JE (reprint author), USGS Earth Resources Observat & Sci EROS Ctr, ASRC Res & Technol Solut ARTS, Sioux Falls, SD 57198 USA.
EM vogel@usgs.gov
RI Chen, Jin/A-6417-2011; li, dongsheng/B-2285-2012; Zhu,
Xiaolin/K-8175-2012; Chen, Jin/I-7666-2016; Chen, Lijun/Q-5012-2016;
OI Chen, Jin/0000-0002-6497-4141; Zhu, Xiaolin/0000-0001-6967-786X;
Vogelmann, James/0000-0002-0804-5823
FU Ministry of Science and Technology of China [2009AA12004]; USGS Landsat
Science Team
FX This study was supported by 863 project (2009AA12004) from Ministry of
Science and Technology of China. We would also like to acknowledge the
support from the USGS Landsat Science Team. We thank Tom Maiersperger,
Kurtis Nelson and an anonymous reviewer for helpful comments on the
manuscript.
NR 20
TC 112
Z9 122
U1 8
U2 51
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR 15
PY 2011
VL 115
IS 4
BP 1053
EP 1064
DI 10.1016/j.rse.2010.12.010
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 728UE
UT WOS:000287899200010
ER
PT J
AU Jones, MO
Jones, LA
Kimball, JS
McDonald, KC
AF Jones, Matthew O.
Jones, Lucas A.
Kimball, John S.
McDonald, Kyle C.
TI Satellite passive microwave remote sensing for monitoring global land
surface phenology
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE AMSR-E; MODIS; Phenology; Optical depth; Vegetation index; NDVI; EVI;
LAI; Growing season
ID POLARIZATION DIFFERENCE INDEX; OPTICAL DEPTH RETRIEVAL; SOIL-MOISTURE;
AMSR-E; VEGETATION INDEXES; SPRING PHENOLOGY; FOREST CANOPY; LEAF-AREA;
EMISSION; BIOMASS
AB Vegetation phenology characterizes seasonal life-cycle events that influence the carbon cycle and land-atmosphere water and energy exchange. We analyzed global phenology cycles over a six year record (2003-2008) using satellite passive microwave remote sensing based Vegetation Optical Depth (VOD) retrievals derived from daily time series brightness temperature (T-b) measurements from the Advanced Microwave Scanning Radiometer on EOS (AMSR-E) and other ancillary data inputs. The VOD parameter derives vegetation canopy attenuation at a given microwave frequency (18.7 GHz) and varies with canopy height, density, structure and water content. An error sensitivity analysis indicates that the retrieval algorithm can resolve the VOD seasonal cycle over a majority of global vegetated land areas. The VOD results corresponded favorably (p < 0.01) with vegetation indices (VIs) and leaf area index (lid) information from satellite optical-infrared (MODIS) remote sensing, and phenology cycles determined from a simple bioclimatic growing season index (GSI) for over 82% of the global domain. Lower biomass land cover classes (e.g. savannas) show the highest correlations (R=0.66), with reduced correspondence at higher biomass levels (0.03 < R < 0.51) and higher correlations for homogeneous land cover areas (0.41 < R < 0.83). The VOD results display a unique end-of-season signal relative to VI and LAI series, and may reflect microwave sensitivity to the timing of vegetation biomass depletion (e.g. leaf abscission) and associated changes in canopy water content (e.g. dormancy preparation). The VOD parameter is independent of and synergistic with optical-infrared remote sensing based vegetation metrics, and contributes to a more comprehensive view of land surface phenology. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Jones, Matthew O.; Jones, Lucas A.; Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA.
[Jones, Matthew O.; Jones, Lucas A.; Kimball, John S.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
[McDonald, Kyle C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jones, MO (reprint author), Univ Montana, Numer Terradynam Simulat Grp, CHCB 424,32 Campus Dr, Missoula, MT 59812 USA.
EM matt.jones@ntsg.umt.edu
FU NASA
FX This study was carried out with funding from the NASA Terrestrial
Ecology program. The AMSR-E Tb data and MODIS land cover in
EASE grid format were provided by the National Snow and Ice Data Center
(NSIDC). Other MODIS data were provided by the EOS data gateway, and NNR
meteorological data were provided by the NOAA/OAR/ESRL PSD, Boulder,
Colorado, USA (http://www.cdc.noaa.gov). The independent emissivity
database was provided by Jean-Luc Moncet and Pan Liang of Atmospheric
and Environmental Research, Inc.,
(http://www.aer.com/scienceResearch/mwrs/emis.html). The AMSR-E global
VOD database and associated biophysical retrievals from this study are
available through the UMT online data archives
(ftp://ftp.ntsg.umt.edu/pub/data) and the NSIDC
(http://nsidc.org/data/nsidc-0451.html). This work was performed at the
University of Montana (UMT) and at the Jet Propulsion Laboratory,
California Institute of Technology, under contract to the National
Aeronautics and Space Administration.
NR 59
TC 79
Z9 81
U1 5
U2 60
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 APR 15
PY 2011
VL 115
IS 4
BP 1102
EP 1114
DI 10.1016/j.rse.2010.12.015
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 728UE
UT WOS:000287899200014
ER
PT J
AU Klima, RL
Pieters, CM
Boardman, JW
Green, RO
Head, JW
Isaacson, PJ
Mustard, JF
Nettles, JW
Petro, NE
Staid, MI
Sunshine, JM
Taylor, LA
Tompkins, S
AF Klima, Rachel L.
Pieters, Carle M.
Boardman, Joseph W.
Green, Robert O.
Head, James W., III
Isaacson, Peter J.
Mustard, John F.
Nettles, Jeff W.
Petro, Noah E.
Staid, Matthew I.
Sunshine, Jessica M.
Taylor, Lawrence A.
Tompkins, Stefanie
TI New insights into lunar petrology: Distribution and composition of
prominent low-Ca pyroxene exposures as observed by the Moon Mineralogy
Mapper (M-3)
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MODIFIED GAUSSIAN MODEL; ORDER-DISORDER; MARE VOLCANISM; EVOLUTION;
SPECTRA; ANORTHOSITES; SPECTROSCOPY; BULLIALDUS; HISTORY; SURFACE
AB Lunar geochemical groups such as Mg suite, ferroan anorthosite, and alkali suite rocks are difficult to distinguish from orbit because they are defined by both modal mineralogy and elemental composition of their constituent minerals. While modal mineralogy can be modeled, only specific minerals or elements can be directly detected. At near-infrared (NIR) wavelengths, pyroxenes are among the most spectrally distinctive minerals, and their absorption bands are sensitive to structure and composition. Pyroxenes thus provide important clues to distinguish these geochemical groups and to understand lunar crustal evolution. Using Moon Mineralogy Mapper data, we search for lithologies dominated by strong low-calcium pyroxene (LCP) signatures. We compare the NIR absorptions of 20 LCPs to a suite of synthetic pyroxenes to determine which lunar pyroxenes appear magnesian enough to be candidate Mg suite norites. We detail three prominent regions of LCP (1) in South Pole-Aitken Basin (SPA), (2) south of Mare Frigoris, and (3) north of Mare Frigoris. The absorption band positions suggest that the LCPs north of Mare Frigoris and those in SPA are compositionally similar to one another and of similar to Mg50-75, implying that the mafic material excavated by the SPA impact was relatively iron-rich. Modified Gaussian modeling results suggest that the Apollo basin may have tapped different composition material than is exposed in much of SPA. The LCPs located in the highlands south of Mare Frigoris exhibit absorption bands at short wavelengths consistent with Mg > similar to 80. The coincidence of these Mg-rich LCPs with the thorium measured by Lunar Prospector make them good candidates for KREEP-related Mg suite pyroxenes.
C1 [Klima, Rachel L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA.
[Pieters, Carle M.; Head, James W., III; Isaacson, Peter J.; Mustard, John F.; Nettles, Jeff W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Boardman, Joseph W.] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA.
[Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Petro, Noah E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Staid, Matthew I.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Taylor, Lawrence A.] Univ Tennessee, Planetary Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Tompkins, Stefanie] Def Adv Res Projects Agcy, Arlington, VA 22203 USA.
RP Klima, RL (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20732 USA.
EM rachel.klima@jhuapl.edu
RI Klima, Rachel/H-9383-2012; Petro, Noah/F-5340-2013
OI Klima, Rachel/0000-0002-9151-6429;
FU NASA [NNM05AB26C]; NASA LSI at the Applied Physics Lab [NNA09D-B31A]
FX We are grateful to Joshua Cahill for a thorough and helpful review that
greatly improved our manuscript. The M3 instrument was funded
as a mission of opportunity through the NASA Discovery program.
M3 science validation is supported through NASA contract
NNM05AB26C. Partial funding for this analysis has also been provided
through NASA LSI at the Applied Physics Lab under contract NNA09D-B31A.
We are extremely grateful to ISRO for the opportunity to fly as a guest
instrument on Chandrayaan-1. The views, opinions, and/or findings
contained in this paper are those of the authors and should not be
interpreted as representing the official views, either expressed or
implied, of the Defense Advanced Research Projects Agency or the
Department of Defense.
NR 50
TC 25
Z9 25
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-PLANET
JI J. Geophys. Res.-Planets
PD APR 14
PY 2011
VL 116
AR E00G06
DI 10.1029/2010JE003719
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 751VV
UT WOS:000289646700002
ER
PT J
AU Verronen, PT
Rodger, CJ
Clilverd, MA
Wang, SH
AF Verronen, Pekka T.
Rodger, Craig J.
Clilverd, Mark A.
Wang, Shuhui
TI First evidence of mesospheric hydroxyl response to electron
precipitation from the radiation belts
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SOLAR PROTON EVENT; NORTHERN-HEMISPHERE; ATMOSPHERE; SATELLITE; NOX
AB Utilizing observations from the Medium Energy Proton and Electron Detector (MEPED) on board the Polar Orbiting Environmental Satellite (POES) and the Microwave Limb Sounder (MLS) on board the Aura satellite, we demonstrate that there is a strong link between 100-300 keV loss cone electron count rates observed in the outer radiation belt and nighttime OH concentrations in the middle mesosphere at 71-78 km altitude. In theory, this can be expected because the ionization caused by energetic electron precipitation (EEP) leads to odd hydrogen (HOx) production through ionic reactions. However, this is the first time that OH production due to EEP has been observed. We consider daily mean data from 2 months, March 2005 and April 2006, which were selected because of (1) relatively high count rates of radiation belt electrons observed and (2) the absence of solar proton events that could mask the EEP effects. The results show that at 55-65 degrees magnetic latitude (equivalent to McIlwain L shells 3.0-5.6) increases in electron count rates by 2 orders of magnitude are accompanied by increases in nighttime OH concentration of 100%. There is a high correlation between MEPED and MLS data such that 56-87% of the OH variation can be explained by changes in EEP. Because the relation between MEPED count rate observations and the flux of electrons actually entering the atmosphere is not trivial, we discuss the possibility of using OH observations to obtain an estimate of EEP forcing that could be used in atmospheric modeling.
C1 [Verronen, Pekka T.] Finnish Meteorol Inst, FI-00101 Helsinki, Finland.
[Rodger, Craig J.] Univ Otago, Dept Phys, Dunedin, New Zealand.
[Clilverd, Mark A.] British Antarctic Survey, Cambridge CB3 0ET, England.
[Wang, Shuhui] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Verronen, PT (reprint author), Finnish Meteorol Inst, POB 503, FI-00101 Helsinki, Finland.
EM pekka.verronen@fmi.fi; crodger@physics.otago.ac.nz; macl@bas.ac.uk;
shuhui.wang@jpl.nasa.gov
RI Verronen, Pekka/G-6658-2014; Rodger, Craig/A-1501-2011
OI Verronen, Pekka/0000-0002-3479-9071; Rodger, Craig/0000-0002-6770-2707
FU Academy of Finland [136225/SPOC, 123275/THERMES]; National Aeronautics
and Space Administration
FX P. T. V. would like to thank Marko Laine for valuable discussions. The
work of P. T. V. was supported by the Academy of Finland through
projects 136225/SPOC (Significance of Energetic Electron Precipitation
to Odd Hydrogen, Ozone, and Climate) and 123275/THERMES (Thermosphere
and Mesosphere Affecting the Stratosphere). Research at the Jet
Propulsion Laboratory, California Institute of Technology, is performed
under contract with the National Aeronautics and Space Administration.
POES data were provided by NOAA National Geophysical Data Center.
MLS/Aura data were provided by the NASA Goddard Earth Sciences Data and
Information Service Center (GES DISC).
NR 27
TC 35
Z9 35
U1 0
U2 5
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 APR 14
PY 2011
VL 116
AR D07307
DI 10.1029/2010JD014965
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 751WI
UT WOS:000289648000003
ER
PT J
AU Hale, AS
Tamppari, LK
Bass, DS
Smith, MD
AF Hale, A. Snyder
Tamppari, L. K.
Bass, D. S.
Smith, M. D.
TI Martian water ice clouds: A view from Mars Global Surveyor Thermal
Emission Spectrometer
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID INTERANNUAL VARIABILITY; MGS TES; VIKING; APHELION; ATMOSPHERE;
BEHAVIOR; CLIMATE; MISSION; ALBEDO; MAPPER
AB We have used the Mars Global Surveyor Thermal Emission Spectrometer (MGS TES) data to map water ice clouds in the Martian atmosphere in the latitude range -60 to +60 over a period of three Martian years. We have used the same method we have previously used on Viking Infrared Thermal Mapper data in order to allow direct comparison of the cloud behavior in the Viking and MGS eras and confirmed the validity of this method by comparing it to MGS TES standard retrievals. We note that the large-scale behavior of water ice clouds is remarkably consistent, both between the Viking and the MGS eras as well as between years observed by MGS. We also compare our results to water ice absorption-only optical depths derived from TES data and show that correlation is best for type 2 water ice clouds.
C1 [Hale, A. Snyder; Tamppari, L. K.; Bass, D. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hale, AS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM amy.s.hale@jpl.nasa.gov
RI Smith, Michael/C-8875-2012
FU NASA
FX The authors would like to thank Charles Thompson for invaluable help in
developing our IDL code and David Paige for the surface model and access
to the source code used to generate it. The authors would like to thank
Alexey Pankine for assistance with estimating the range of appropriate
cloud temperatures within the TES data set; they would also like to
thank Terry Z. Martin and Deborah Bass for many helpful discussions and
Ashwin Vasavada for his comments on a draft version of this paper. This
work was carried out at JPL/CIT under a grant from the NASA Mars Data
Analysis Program. We would also like to thank Sasha Rodin and an
anonymous reviewer for their helpful comments and critique, which have
greatly improved this manuscript.
NR 29
TC 1
Z9 1
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR 13
PY 2011
VL 116
AR E04004
DI 10.1029/2009JE003449
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 751VT
UT WOS:000289646500001
ER
PT J
AU Heavens, NG
Richardson, MI
Kleinbohl, A
Kass, DM
McCleese, DJ
Abdou, W
Benson, JL
Schofield, JT
Shirley, JH
Wolkenberg, PM
AF Heavens, N. G.
Richardson, M. I.
Kleinboehl, A.
Kass, D. M.
McCleese, D. J.
Abdou, W.
Benson, J. L.
Schofield, J. T.
Shirley, J. H.
Wolkenberg, P. M.
TI The vertical distribution of dust in the Martian atmosphere during
northern spring and summer: Observations by the Mars Climate Sounder and
analysis of zonal average vertical dust profiles
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; WATER ICE CLOUDS; MIDDLE ATMOSPHERE; ORBITER
CAMERA; INTERANNUAL VARIABILITY; INFRARED MEASUREMENTS; THERMAL
STRUCTURE; POLAR WARMINGS; PARTICLE SIZES; MGS TES
AB The vertical distribution of dust in Mars's atmosphere is a critical and poorly known input in atmospheric physical and chemical models and a source of insight into the lifting and transport of dust and general vertical mixing in the atmosphere. We investigate vertical profiles of dust opacity retrieved from limb observations by Mars Climate Sounder during the relatively dust-clear Martian northern summer of 2006-2007 (L-s = 111 degrees-177 degrees of Mars year (MY) 28) and Martian northern spring and summer of 2007-2008 (L-s = 0 degrees-180 degrees of MY 29). To represent local maxima in inferred mass mixing ratio in these profiles, we develop an empirical alternative to the classic "Conrath profile" for representing the vertical distribution of dust in the Martian atmosphere. We then assess the magnitude and variability of atmospheric dust loading, the depth of dust penetration during these seasons, and the impact of the observed vertical dust distribution on the radiative forcing of the circulation. During most of northern spring and summer, the dust mass mixing ratio in the tropics has a maximum at 15-25 km above the local surface (the high-altitude tropical dust maximum (HATDM)). The HATDM appears to have increased significantly in magnitude and altitude during middle to late northern summer of MY 29. The HATDM gradually decayed during late summer of MY 28. Interannual variability in the dust distribution during middle to late northern summer may be connected with known interannual variability in tropical dust storm activity.
C1 [Richardson, M. I.] Ashima Res, Pasadena, CA 91106 USA.
[Heavens, N. G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA.
[Kleinboehl, A.; Kass, D. M.; McCleese, D. J.; Abdou, W.; Benson, J. L.; Schofield, J. T.; Shirley, J. H.; Wolkenberg, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Heavens, NG (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, 1118 Bradfield Hall, Ithaca, NY 14853 USA.
EM heavens@cornell.edu
OI Heavens, Nicholas/0000-0001-7654-503X
FU National Aeronautics and Space Administration
FX We thank Aymeric Spiga and an anonymous reviewer for extremely thorough
and helpful reviews. The authors also would like to thank Tim
McConnochie and Todd Clancy for useful discussions. This work was funded
by and performed in part at the Jet Propulsion Laboratory, California
Institute of Technology under contract with the National Aeronautics and
Space Administration as part of the Mars Reconnaissance Orbiter project.
NR 64
TC 32
Z9 32
U1 0
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR 13
PY 2011
VL 116
AR E04003
DI 10.1029/2010JE003691
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 751VT
UT WOS:000289646500002
ER
PT J
AU Hwang, KJ
Goldstein, ML
Lee, E
Pickett, JS
AF Hwang, K. -J.
Goldstein, M. L.
Lee, E.
Pickett, J. S.
TI Cluster observations of multiple dipolarization fronts
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PROTON-BEAM GENERATION; WHISTLER WAVES; MAGNETIC RECONNECTION; CURRENT
DISRUPTION; EARTH; MAGNETOSPHERE; INSTABILITY; MOTION; FLOWS; SHEET
AB We present Cluster observations of a series of dipolarization fronts (DF 1 to 6) at the central current sheet in Earth's magnetotail. The velocities of fast earthward flow following behind each DF 1-3 are comparable to the Alfven velocity, indicating that the flow bursts might have been generated by bursty reconnection that occurred tailward of the spacecraft. Based on multispacecraft timing analysis, DF normals are found to propagate mainly earthward at 160-335 km/s with a thickness of 900-1500 km, which corresponds to the ion inertial length or gyroradius scale. Each DF is followed by significant fluctuations in the x and y components of the magnetic field whose peaks are found 1-2 min after the DF passage. These (B-x, B-y) fluctuations propagate dawnward (mainly) and earthward. Strongly enhanced field-aligned beams are observed coincidently with (B-x, B-y) fluctuations, while an enhancement of cross-tail currents is associated with the DFs. From the observed pressure imbalance and flux tube entropy changes between the two regions separated by the DF, we speculate that interchange instability destabilizes the DFs and causes the deformation of the midtail magnetic topology. This process generates significant field-aligned currents and might power the auroral brightening in the ionosphere. However, this event is associated with neither the main substorm auroral breakup nor the poleward expansion, which might indicate that the observed multiple DFs have been dissipated before they reach the inner plasma sheet boundary.
C1 [Hwang, K. -J.; Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lee, E.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Kyung Ki, South Korea.
[Pickett, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Hwang, K. -J.] Univ Maryland Baltimore Cty, Goddard Earth & Sci Technol Ctr, Baltimore, MD 21228 USA.
RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
EM kyoung-joo.hwang@nasa.gov; melvyn.l.goldstein@nasa.gov; eslee@khu.ac.kr;
pickett@uiowa.edu
RI Goldstein, Melvyn/B-1724-2008; Lee, Ensang/E-2356-2013; NASA MMS,
Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA's MMS/IDS and Cluster missions at the Goddard Space Flight Center;
UMBC/GEST
FX This study was supported by NASA's MMS/IDS and Cluster missions at the
Goddard Space Flight Center and by UMBC/GEST. We acknowledges all
Cluster instrument teams, including PEACE, CIS, FGM, EFW, RAPID,
WHISPER, and WIDEBAND staffs and the Cluster Active Archive
(http://caa.estec.esa.int/caa). The authors acknowledge the referee
correcting the estimation of the foot point of the Cluster location
using the T96 model and both referee advising in using the
interchange-instability criterion. K.-J. Hwang thanks Miho Saito for
helpful discussions.
NR 57
TC 36
Z9 36
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 APR 13
PY 2011
VL 116
AR A00I32
DI 10.1029/2010JA015742
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 751VG
UT WOS:000289645200002
ER
PT J
AU Lau, KM
Kim, KM
AF Lau, K. M.
Kim, K. M.
TI Comment on '"Elevated heat pump' hypothesis for the aerosol-monsoon
hydroclimate link: 'Grounded' in observations?" by S. Nigam and M.
Bollasina
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Editorial Material
ID BLACK CARBON AEROSOLS; ASIAN SUMMER MONSOON; INDIAN MONSOON
C1 [Lau, K. M.] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kim, K. M.] Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Baltimore, MD 21250 USA.
RP Lau, KM (reprint author), NASA, Atmospheres Lab, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
EM william.k.lau@nasa.gov
RI Kim, Kyu-Myong/G-5398-2014; Lau, William /E-1510-2012
OI Lau, William /0000-0002-3587-3691
NR 11
TC 16
Z9 17
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 12
PY 2011
VL 116
AR D07203
DI 10.1029/2010JD014800
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 751WG
UT WOS:000289647800001
ER
PT J
AU Jenet, FA
Armstrong, JW
Tinto, M
AF Jenet, Fredrick A.
Armstrong, J. W.
Tinto, Massimo
TI Pulsar timing sensitivity to very-low-frequency gravitational waves
SO PHYSICAL REVIEW D
LA English
DT Article
ID BLACK-HOLE BINARIES; UPPER LIMITS; RADIATION; COALESCENCE; PRECISION;
MODEL
AB We compute the sensitivity, constrained by instrumental, propagation, and other fundamental noises, of pulsar timing to very-low-frequency gravitational waves (GWs). Reaching predicted GW signal strengths will require suppression of time-of-arrival fluctuations caused by interstellar plasma turbulence and a reduction of white rms timing noise to less than or similar to 100 ns. Assuming negligible intrinsic pulsar rotational noise, perfect time transfer from time standard to observatory, and stable pulse profiles, the resulting single-pulsar signal-to-noise ratio 1 sensitivity is limited by terrestrial time standards at h(rms) similar to 2 x 10(-16) [f/(1 cycle/year)] -1/2 for f < 3 x 10(-8) Hz, where f is the Fourier frequency and a bandwidth of 1 cycle/(10 years) is assumed. Since this sensitivity is comparable to predicted GW signal levels, a reliable detection will require substantial signal-to-noise ratio improvement via pulsar timing array.
C1 [Jenet, Fredrick A.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
[Armstrong, J. W.; Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jenet, FA (reprint author), Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
EM merlyn@phys.utb.edu; john.w.armstrong@jpl.nasa.gov;
massimo.tinto@jpl.nasa.gov
FU U.S. National Science Foundation (AST) [0545837]; National Aeronautics
and Space Administration; internal Research and Technology Development
program
FX We thank F. B. Estabrook for discussions on gravitational wave
sensitivity and W. A. Coles for comments on an early draft of this
paper. F. A. J.'s contribution was funded by a grant from the U.S.
National Science Foundation (AST #0545837). For J. W. A. and M. T., this
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration and funded through the internal Research and
Technology Development program.
NR 32
TC 8
Z9 8
U1 0
U2 1
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 APR 11
PY 2011
VL 83
IS 8
AR 081301
DI 10.1103/PhysRevD.83.081301
PG 4
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 747WZ
UT WOS:000289353200001
ER
PT J
AU Garcia, J
Ramirez, JM
Kallman, TR
Witthoeft, M
Bautista, MA
Mendoza, C
Palmeri, P
Quinet, P
AF Garcia, J.
Ramirez, J. M.
Kallman, T. R.
Witthoeft, M.
Bautista, M. A.
Mendoza, C.
Palmeri, P.
Quinet, P.
TI MODELING THE OXYGEN K ABSORPTION IN THE INTERSTELLAR MEDIUM: AN
XMM-NEWTON VIEW OF Sco X-1
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE atomic data; atomic processes; dust, extinction; line: formation;
X-rays: general
ID X-RAY SPECTROSCOPY; FINE-STRUCTURE; ATOMIC OXYGEN; SCORPIUS X-1; EDGE;
IRON; PHOTOABSORPTION; MCG-6-30-15; SPECTRUM; DUST
AB We investigate the X-ray absorption structure of oxygen in the interstellar medium by analyzing XMM-Newton observations of the low-mass X-ray binary Sco X-1. Simple models based on the O I atomic photoabsorption cross section from different sources are used to fit the data and evaluate the impact of the atomic data on the interpretation of the observations. We show that relatively small differences in the atomic calculations can yield spurious results, and that the most complete and accurate set of atomic cross sections successfully reproduce the observed data in the 21.0-24.5 angstrom wavelength region of the spectrum. Our fits indicate that the absorption is mainly due to neutral gas with an ionization parameter of xi = 10(-4) erg cm s(-1) and an oxygen column density of N-O approximate to (8-10) x 10(17) cm(-2). The models are able to reproduce both the K edge and the K alpha absorption line from O I which are the two main features in this region. We find no conclusive evidence for absorption by anything other than atomic oxygen.
C1 [Garcia, J.; Bautista, M. A.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Garcia, J.; Kallman, T. R.; Witthoeft, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ramirez, J. M.] Inst Astrophys, D-14482 Potsdam, Germany.
[Mendoza, C.] IVIC, Ctr Fis, Caracas 1020, Venezuela.
[Palmeri, P.; Quinet, P.] Univ Mons, B-7000 Mons, Belgium.
[Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium.
RP Garcia, J (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
EM javier.garcia@wmich.edu; jramirez@aip.de; timothy.r.kallman@nasa.gov;
michael.c.witthoeft@nasa.gov; manuel.bautista@wmich.edu;
claudio@ivic.gob.ve; palmeri@umh.ac.be; quinet@umh.ac.be
FU NASA [05-ATP05-18]
FX We thank Tom Gorczyca for providing the MCK98 and GMC00 calculations.
This work was supported by a grant from the NASA astrophysics theory
program 05-ATP05-18. This research has made extensive use of the NASA
Astrophysics Data System.
NR 32
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U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2011
VL 731
IS 1
AR L15
DI 10.1088/2041-8205/731/1/L15
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797KQ
UT WOS:000293126600015
ER
PT J
AU Miller, JM
Maitra, D
Cackett, EM
Bhattacharyya, S
Strohmayer, TE
AF Miller, Jon M.
Maitra, Dipankar
Cackett, Edward M.
Bhattacharyya, Sudip
Strohmayer, Tod E.
TI A FAST X-RAY DISK WIND IN THE TRANSIENT PULSAR IGR J17480-2446 IN TERZAN
5
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; globular clusters: individual (Terzan 5);
pulsars: individual (IGR J17480-2446); stars: neutron
ID ACCRETION DISKS; NEUTRON-STAR; MILLISECOND PULSAR; SAX J1808.4-3658;
CHANDRA; LINES; SPECTROSCOPY; BINARIES; DISCOVERY; EMISSION
AB Accretion disk winds are revealed in Chandra gratings spectra of black holes. The winds are hot and highly ionized (typically composed of He-like and H-like charge states) and show modest blueshifts. Similar line spectra are sometimes seen in "dipping" low-mass X-ray binaries (LMXBs), which are likely viewed edge-on; however, that absorption is tied to structures in the outer disk, and blueshifts are not typically observed. Here, we report the detection of blueshifted He-like Fe XXV (3100 +/- 400 km s(-1)) and H-like Fe XXVI (1000 +/- 200 km s(-1)) absorption lines in a Chandra/HETG spectrum of the transient pulsar and LMXB IGR J17480-2446 in Terzan 5. These features indicate a disk wind with at least superficial similarities to those observed in stellar-mass black holes. The wind does not vary strongly with numerous weak X-ray bursts or flares. A broad Fe K emission line is detected in the spectrum, and fits with different line models suggest that the inner accretion disk in this system may be truncated. If the stellar magnetic field truncates the disk, a field strength of B = (0.7-4.0) x 10(9) G is implied, which is in line with estimates based on X-ray timing techniques. We discuss our findings in the context of accretion flows onto neutron stars and stellar-mass black holes.
C1 [Miller, Jon M.; Maitra, Dipankar] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Cackett, Edward M.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Bhattacharyya, Sudip] Tata Inst Fundamental Res, Dept Astron & Astrophys, Mumbai 400005, Maharashtra, India.
[Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM jonmm@umich.edu
FU Chandra Guest Observer program
FX We thank Harvey Tananbaum, Belinda Wilkes, and Andrea Prestwich for
executing this observation. We acknowledge David Pooley and Jeroen Homan
for helping to coordinate different observations of IGR J17480-2446. We
thank Tim Kallman and Cole Miller for helpful discussions. Finally, we
thank the anonymous referee for a helpful review. J.M.M. acknowledges
support from the Chandra Guest Observer program.
NR 40
TC 35
Z9 35
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2011
VL 731
IS 1
AR L7
DI 10.1088/2041-8205/731/1/L7
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797KQ
UT WOS:000293126600007
ER
PT J
AU Moore, RL
Sterling, AC
Cirtain, JW
Falconer, DA
AF Moore, Ronald L.
Sterling, Alphonse C.
Cirtain, Jonathan W.
Falconer, David A.
TI SOLAR X-RAY JETS, TYPE-II SPICULES, GRANULE-SIZE EMERGING BIPOLES, AND
THE GENESIS OF THE HELIOSPHERE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: chromosphere; Sun: corona; Sun: heliosphere; Sun:
magnetic topology; Sun: surface magnetism
ID HORIZONTAL MAGNETIC-FIELDS; QUIET-SUN INTERNETWORK; CORONAL JETS;
ENERGY-FLOW; CHROMOSPHERE; TELESCOPE; MODEL; NETWORK; REGIONS; WAVES
AB From Hinode observations of solar X-ray jets, Type-II spicules, and granule-size emerging bipolar magnetic fields in quiet regions and coronal holes, we advocate a scenario for powering coronal heating and the solar wind. In this scenario, Type-II spicules and Alfven waves are generated by the granule-size emerging bipoles (EBs) in the manner of the generation of X-ray jets by larger magnetic bipoles. From observations and this scenario, we estimate that Type-II spicules and their co-generated Alfven waves carry into the corona an area-average flux of mechanical energy of similar to 7 x 10(5) erg cm(-2) s(-1). This is enough to power the corona and solar wind in quiet regions and coronal holes, and therefore indicates that the granule-size EBs are the main engines that generate and sustain the entire heliosphere.
C1 [Moore, Ronald L.; Sterling, Alphonse C.; Cirtain, Jonathan W.; Falconer, David A.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
[Falconer, David A.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Falconer, David A.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
RP Moore, RL (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
EM ron.moore@nasa.gov
FU NASA's Science Mission Directorate
FX This work was funded by NASA's Science Mission Directorate through the
Heliophysics Guest Investigators Program, the Hinode Project, and the
Living With a Star Targeted Research and Technology Program.
NR 43
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U2 9
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 APR 10
PY 2011
VL 731
IS 1
AR L18
DI 10.1088/2041-8205/731/1/L18
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797KQ
UT WOS:000293126600018
ER
PT J
AU Sterling, AC
Moore, RL
Freeland, SL
AF Sterling, Alphonse C.
Moore, Ronald L.
Freeland, Samuel L.
TI INSIGHTS INTO FILAMENT ERUPTION ONSET FROM SOLAR DYNAMICS OBSERVATORY
OBSERVATIONS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: filaments, prominences; Sun: flares; Sun: UV
radiation
ID CORONAL MASS EJECTIONS; UNSTABLE FLUX ROPES; EMERGING FLUX;
MAGNETIC-FLUX; SLOW-RISE; FLARES; INITIATION; HINODE; RECONNECTION;
CANCELLATION
AB We examine the buildup to and onset of an active region filament confined eruption of 2010 May 12, using EUV imaging data from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Array and line-of-sight magnetic data from the SDO Helioseismic and Magnetic Imager. Over the hour preceding eruption the filament undergoes a slow rise averaging similar to 3 km s(-1), with a step-like trajectory. Accompanying a final rise step similar to 20 minutes prior to eruption is a transient preflare brightening, occurring on loops rooted near the site where magnetic field had canceled over the previous 20 hr. Flow-type motions of the filament are relatively smooth with speeds similar to 50 km s(-1) prior to the preflare brightening and appear more helical, with speeds similar to 50-100 km s(-1), after that brightening. After a final plateau in the filament's rise, its rapid eruption begins, and concurrently an outer shell "cocoon" of the filament material increases in emission in hot EUV lines, consistent with heating in a newly formed magnetic flux rope. The main flare brightenings start similar to 5 minutes after eruption onset. The main flare arcade begins between the legs of an envelope-arcade loop that is nearly orthogonal to the filament, suggesting that the flare results from reconnection among the legs of that loop. This progress of events is broadly consistent with flux cancellation leading to formation of a helical flux rope that subsequently erupts due to onset of a magnetic instability and/or runaway tether cutting.
C1 [Sterling, Alphonse C.; Moore, Ronald L.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
[Freeland, Samuel L.] Lockheed Martin Solar & Astrophys Lab, Dept ADBS, Palo Alto, CA 94304 USA.
RP Sterling, AC (reprint author), JAXA, Inst Space & Astronaut Sci, Hinode Grp, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov
FU NASA's Office of Space Science
FX We thank G. L. Slater for valuable assistance with the AIA data. SDO is
a mission for NASA's Living With a Star (LWS) Program. A. C. S. and R.
L. M. were supported by funding from NASA's Office of Space Science
through the Solar Physics Supporting Research and Technology Program,
the Sun-Earth Connection Guest Investigator Program, and the Living With
a Star Targeted Research & Technology Program.
NR 50
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U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2011
VL 731
IS 1
AR L3
DI 10.1088/2041-8205/731/1/L3
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797KQ
UT WOS:000293126600003
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bonamente, E
Borgland, AW
Bouvier, A
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Carrigan, S
Casandjian, JM
Cavazzuti, E
Cecchi, C
Celik, O
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Costamante, L
Cutini, S
Davis, DS
Dermer, CD
de Palma, F
Digel, SW
Silva, EDE
Drell, PS
Dubois, R
Dumora, D
Favuzzi, C
Fegan, SJ
Fortin, P
Frailis, M
Fuhrmann, L
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guillemot, L
Guiriec, S
Hadasch, D
Hayashida, M
Hays, E
Horan, D
Hughes, RE
Itoh, R
Johannesson, G
Johnson, AS
Johnson, TJ
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Makeev, A
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Naumann-Godo, M
Nestoras, I
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Reyes, LC
Ripken, J
Ritz, S
Romani, RW
Roth, M
Sadrozinski, HFW
Sanchez, D
Sander, A
Scargle, JD
Sgro, C
Shaw, MS
Smith, PD
Spandre, G
Spinelli, P
Strickman, MS
Suson, DJ
Takahashi, H
Tanaka, T
Thayer, JB
Thayer, JG
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Tramacere, A
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vilchez, N
Vitale, V
Waite, AP
Wang, P
Winer, BL
Wood, KS
Yang, Z
Ylinen, T
Ziegler, M
Acciari, VA
Aliu, E
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bottcher, M
Boltuch, D
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Christiansen, JL
Ciupik, L
Cui, W
Perez, ID
Dickherber, R
Errando, M
Falcone, A
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Hui, CM
Humensky, TB
Imran, A
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Konopelko, A
Krawczynski, H
Krennrich, F
Lang, MJ
LeBohec, S
Maier, G
McArthur, S
McCann, A
McCutcheon, M
Moriarty, P
Mukherjee, R
Ong, RA
Otte, AN
Pandel, D
Perkins, JS
Pichel, A
Pohl, M
Quinn, J
Ragan, K
Reynolds, PT
Roache, E
Rose, HJ
Schroedter, M
Sembroski, GH
Senturk, GD
Smith, AW
Steele, D
Swordy, SP
Tesic, G
Theiling, M
Thibadeau, S
Varlotta, A
Vassiliev, VV
Vincent, S
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Wissel, S
Wood, M
Villata, M
Raiteri, CM
Gurwell, MA
Larionov, VM
Kurtanidze, OM
Aller, MF
Lahteenmaki, A
Chen, WP
Berduygin, A
Agudo, I
Aller, HD
Arkharov, AA
Bach, U
Bachev, R
Beltrame, P
Benitez, E
Buemi, CS
Dashti, J
Calcidese, P
Capezzali, D
Carosati, D
Da Rio, D
Di Paola, A
Diltz, C
Dolci, M
Dultzin, D
Forne, E
Gomez, JL
Hagen-Thorn, VA
Halkola, A
Heidt, J
Hiriart, D
Hovatta, T
Hsiao, HY
Jorstad, SG
Kimeridze, GN
Konstantinova, TS
Kopatskaya, EN
Koptelova, E
Leto, P
Ligustri, R
Lindfors, E
Lopez, JM
Marscher, AP
Mommert, M
Mujica, R
Nikolashvili, MG
Nilsson, K
Palma, N
Pasanen, M
Roca-Sogorb, M
Ros, JA
Roustazadeh, P
Sadun, AC
Saino, J
Sigua, LA
Sillanaa, A
Sorcia, M
Takalo, LO
Tornikoski, M
Trigilio, C
Turchetti, R
Umana, G
Belloni, T
Blake, CH
Bloom, JS
Angelakis, E
Fumagalli, M
Hauser, M
Prochaska, JX
Riquelme, D
Sievers, A
Starr, DL
Tagliaferri, G
Ungerechts, H
Wagner, S
Zensus, JA
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Carrigan, S.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Celik, Oe.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Costamante, L.
Cutini, S.
Davis, D. S.
Dermer, C. D.
de Palma, F.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Dubois, R.
Dumora, D.
Favuzzi, C.
Fegan, S. J.
Fortin, P.
Frailis, M.
Fuhrmann, L.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guillemot, L.
Guiriec, S.
Hadasch, D.
Hayashida, M.
Hays, E.
Horan, D.
Hughes, R. E.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Johnson, T. J.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Makeev, A.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mizuno, T.
Moiseev, A. A.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Naumann-Godo, M.
Nestoras, I.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Reyes, L. C.
Ripken, J.
Ritz, S.
Romani, R. W.
Roth, M.
Sadrozinski, H. F. -W.
Sanchez, D.
Sander, A.
Scargle, J. D.
Sgro, C.
Shaw, M. S.
Smith, P. D.
Spandre, G.
Spinelli, P.
Strickman, M. S.
Suson, D. J.
Takahashi, H.
Tanaka, T.
Thayer, J. B.
Thayer, J. G.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Tramacere, A.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vilchez, N.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Ylinen, T.
Ziegler, M.
Acciari, V. A.
Aliu, E.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Boettcher, M.
Boltuch, D.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Christiansen, J. L.
Ciupik, L.
Cui, W.
de la Calle Perez, I.
Dickherber, R.
Errando, M.
Falcone, A.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Godambe, S.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Hui, C. M.
Humensky, T. B.
Imran, A.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Konopelko, A.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
LeBohec, S.
Maier, G.
McArthur, S.
McCann, A.
McCutcheon, M.
Moriarty, P.
Mukherjee, R.
Ong, R. A.
Otte, A. N.
Pandel, D.
Perkins, J. S.
Pichel, A.
Pohl, M.
Quinn, J.
Ragan, K.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Schroedter, M.
Sembroski, G. H.
Senturk, G. Demet
Smith, A. W.
Steele, D.
Swordy, S. P.
Tesic, G.
Theiling, M.
Thibadeau, S.
Varlotta, A.
Vassiliev, V. V.
Vincent, S.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
Wissel, S.
Wood, M.
Villata, M.
Raiteri, C. M.
Gurwell, M. A.
Larionov, V. M.
Kurtanidze, O. M.
Aller, M. F.
Laehteenmaeki, A.
Chen, W. P.
Berduygin, A.
Agudo, I.
Aller, H. D.
Arkharov, A. A.
Bach, U.
Bachev, R.
Beltrame, P.
Benitez, E.
Buemi, C. S.
Dashti, J.
Calcidese, P.
Capezzali, D.
Carosati, D.
Da Rio, D.
Di Paola, A.
Diltz, C.
Dolci, M.
Dultzin, D.
Forne, E.
Gomez, J. L.
Hagen-Thorn, V. A.
Halkola, A.
Heidt, J.
Hiriart, D.
Hovatta, T.
Hsiao, H. -Y.
Jorstad, S. G.
Kimeridze, G. N.
Konstantinova, T. S.
Kopatskaya, E. N.
Koptelova, E.
Leto, P.
Ligustri, R.
Lindfors, E.
Lopez, J. M.
Marscher, A. P.
Mommert, M.
Mujica, R.
Nikolashvili, M. G.
Nilsson, K.
Palma, N.
Pasanen, M.
Roca-Sogorb, M.
Ros, J. A.
Roustazadeh, P.
Sadun, A. C.
Saino, J.
Sigua, L. A.
Sillanaa, A.
Sorcia, M.
Takalo, L. O.
Tornikoski, M.
Trigilio, C.
Turchetti, R.
Umana, G.
Belloni, T.
Blake, C. H.
Bloom, J. S.
Angelakis, E.
Fumagalli, M.
Hauser, M.
Prochaska, J. X.
Riquelme, D.
Sievers, A.
Starr, D. L.
Tagliaferri, G.
Ungerechts, H.
Wagner, S.
Zensus, J. A.
CA Fermi-LAT Collaboration
VERITAS Collaboration
GASP-WEBT Consortium
TI MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING GAMMA-RAY BLAZAR 3C 66A IN
2008 OCTOBER (vol 726, pg 43, 2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Shaw, M. S.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Abdo, A. A.; Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Brez, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Shaw, M. S.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Tibaldo, L.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ 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.; Horan, D.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] Sci Data Ctr, ASI, I-00044 Rome, Italy.
[Celik, Oe.; Davis, D. S.; Gehrels, N.; Hays, E.; Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe.; Moiseev, A. A.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe.; Davis, D. S.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe.; Davis, D. S.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France.
[Conrad, J.; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Ripken, J.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Dumora, D.; Guillemot, L.; Lott, B.] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France.
[Dumora, D.; Guillemot, L.; Lott, B.] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France.
[Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fuhrmann, L.; Guillemot, L.; Nestoras, I.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Fukazawa, Y.; Itoh, R.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama Huntsville, CSPAR, Huntsville, AL 35899 USA.
[Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.; Vilchez, N.] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[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.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.] 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.
[Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden.
[Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA.
[Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Boettcher, M.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA.
[Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Byrum, K.; Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Christiansen, J. L.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[de la Calle Perez, I.] Satellite Tracking Stn, European Space Astron Ctr INSA ESAC, ESA, E-28080 Madrid, Spain.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Villata, M.; Raiteri, C. M.] Osserv Astron Torino, INAF, Turin, Italy.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Boston, MA USA.
[Larionov, V. M.; Hagen-Thorn, V. A.; Konstantinova, T. S.; Kopatskaya, E. N.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Larionov, V. M.; Hagen-Thorn, V. A.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia.
[Kurtanidze, O. M.; Kimeridze, G. N.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia.
[Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Laehteenmaeki, A.; Hovatta, T.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Helsinki, Finland.
[Chen, W. P.; Hsiao, H. -Y.; Koptelova, E.] Natl Cent Univ, Inst Astron, Taipei, Taiwan.
[Berduygin, A.; Halkola, A.; Lindfors, E.; Pasanen, M.; Saino, J.; Sillanaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, Dept Phys & Astron, SF-20500 Turku, Finland.
[Agudo, I.; Gomez, J. L.; Roca-Sogorb, M.] CSIC, Inst Astrofis Andalucia, Madrid, Spain.
[Bachev, R.] Bulgarian Acad Sci, Inst Astron, BG-1040 Sofia, Bulgaria.
[Benitez, E.; Dultzin, D.; Sorcia, M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, Catania, Italy.
[Dashti, J.; Diltz, C.; Palma, N.; Roustazadeh, P.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA.
[Calcidese, P.] Osservatorio Astron Reg Autonoma Aosta, Aosta, Italy.
[Di Paola, A.] Osserv Astron Roma, INAF, Rome, Italy.
[Dolci, M.] Osservatorio Astron Collurania Teramo, INAF, Teramo, Italy.
[Forne, E.; Ros, J. A.] Agrupacio Astron Sabadell, Sabadell, Spain.
[Heidt, J.; Mommert, M.] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany.
[Hiriart, D.; Lopez, J. M.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico.
[Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Mommert, M.] Inst Planetary Res, DLR, D-12489 Berlin, Germany.
[Mujica, R.] INAOE, Puebla 72000, Mexico.
[Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
[Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80202 USA.
[Belloni, T.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Blake, C. H.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Bloom, J. S.; Starr, D. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Angelakis, E.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Fumagalli, M.; Prochaska, J. X.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Hauser, M.; Wagner, S.] Heidelberg Univ, D-69117 Heidelberg, Germany.
[Prochaska, J. X.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Riquelme, D.; Sievers, A.; Ungerechts, H.] Inst Radio Astron Millimetr, Granada 18012, Spain.
[Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden.
RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM lreyes@kicp.uchicago.edu
RI Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson,
Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Agudo, Ivan/G-1701-2015;
Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013;
Hagen-Thorn, Vladimir/H-3983-2013; Loparco, Francesco/O-8847-2015;
Gargano, Fabio/O-8934-2015; Johannesson, Gudlaugur/O-8741-2015;
Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Thompson,
David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery,
Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano,
pasquale/F-7269-2012; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Reimer,
Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013;
Kopatskaya, Evgenia/H-4720-2013; 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; Funk, Stefan/B-7629-2015
OI Agudo, Ivan/0000-0002-3777-6182; Jorstad, Svetlana/0000-0001-9522-5453;
Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn,
Vladimir/0000-0002-6431-8590; Loparco, Francesco/0000-0002-1173-5673;
Gargano, Fabio/0000-0002-5055-6395; Johannesson,
Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672; Thompson,
David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806;
giglietto, nicola/0000-0002-9021-2888; Morselli,
Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Larionov,
Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X;
Torres, Diego/0000-0002-1522-9065; Funk, Stefan/0000-0002-2012-0080
NR 2
TC 3
Z9 3
U1 0
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2011
VL 731
IS 1
AR 77
DI 10.1088/0004-637X/731/1/77
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800077
ER
PT J
AU Bell, TA
Willacy, K
Phillips, TG
Allen, M
Lis, DC
AF Bell, T. A.
Willacy, K.
Phillips, T. G.
Allen, M.
Lis, D. C.
TI THE INFLUENCE OF DEUTERATION AND TURBULENT DIFFUSION ON THE OBSERVED D/H
RATIO
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; diffusion; ISM: abundances; ISM: clouds; ISM: molecules;
turbulence
ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; PRE-PROTOSTELLAR COLLAPSE; DENSE
INTERSTELLAR CORES; DEUTERIUM FRACTIONATION; MOLECULAR CLOUDS;
PRESTELLAR CORES; CO DEPLETION; GALACTIC DISK; 1ST DETECTION; DARK
CLOUDS
AB The influence of turbulent mixing on the chemistry of the interstellar medium (ISM) has so far received little attention. Previous studies of this effect have suggested that it might play an important role in mixing the various phases of the ISM. In this paper, we examine the potential effects of turbulent diffusion on the deuterium chemistry within molecular clouds. We find that such mixing acts to reduce the efficiency of deuteration in these clouds by increasing the ionization fraction and reducing freeze-out of heavy molecules. This leads to lower abundances for many deuterated species. We also examine the influence of turbulent mixing on the transition from atomic hydrogen to H-2 and from atomic deuterium to HD near the cloud edge. We find that including turbulent diffusion in our models serves to push these transitions deeper into the cloud and helps maintain a higher atomic fraction throughout the cloud envelope. Based on these findings, we propose a new process to account for the significant scatter in the observed atomic D/H ratio for galactic sightlines extending beyond the Local Bubble. Although several mechanisms have been put forward to explain this scatter, they are unable to fully account for the range in D/H values. We suggest a scenario in which turbulent mixing of atomic and molecular gas at the edges of molecular clouds causes the observed atomic D/H ratio to vary by a factor of similar to 2.
C1 [Bell, T. A.; Phillips, T. G.; Lis, D. C.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Willacy, K.; Allen, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bell, TA (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM tab@caltech.edu
FU National Science Foundation [AST-0838261]; National Aeronautics and
Space Administration
FX We thank W. D. Langer for helpful discussions and the referee for
constructive comments which helped to improve an earlier draft of this
paper. This research has been supported by the National Science
Foundation grant AST-0838261 to the Caltech Submillimeter Observatory.
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 78
TC 6
Z9 6
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2011
VL 731
IS 1
AR 48
DI 10.1088/0004-637X/731/1/48
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800048
ER
PT J
AU Chiar, JE
Pendleton, YJ
Allamandola, LJ
Boogert, ACA
Ennico, K
Greene, TP
Geballe, TR
Keane, JV
Lada, CJ
Mason, RE
Roellig, TL
Sandford, SA
Tielens, AGGM
Werner, MW
Whittet, DCB
Decin, L
Eriksson, K
AF Chiar, J. E.
Pendleton, Y. J.
Allamandola, L. J.
Boogert, A. C. A.
Ennico, K.
Greene, T. P.
Geballe, T. R.
Keane, J. V.
Lada, C. J.
Mason, R. E.
Roellig, T. L.
Sandford, S. A.
Tielens, A. G. G. M.
Werner, M. W.
Whittet, D. C. B.
Decin, L.
Eriksson, K.
TI ICES IN THE QUIESCENT IC 5146 DENSE CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; dust, extinction; infrared: ISM; ISM: individual objects
(IC 5146); ISM: molecules
ID TAURUS DARK CLOUDS; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS;
DIFFUSE INTERSTELLAR-MEDIUM; SOLID CARBON-MONOXIDE; 3 MICRON SPECTRA;
INFRARED-SPECTROSCOPY; MOLECULAR-CLOUD; ABSORPTION FEATURES; ABSOLUTE
CALIBRATION
AB This paper presents spectra in the 2 to 20 mu m range of quiescent cloud material located in the IC 5146 cloud complex. The spectra were obtained with NASA's Infrared Telescope Facility SpeX instrument and the Spitzer Space Telescope's Infrared Spectrometer. We use these spectra to investigate dust and ice absorption features in pristine regions of the cloud that are unaltered by embedded stars. We find that the H2O-ice threshold extinction is 4.03 +/- 0.05 mag. Once foreground extinction is taken into account, however, the threshold drops to 3.2 mag, equivalent to that found for the Taurus dark cloud, generally assumed to be the touchstone quiescent cloud against which all other dense cloud and embedded young stellar object observations are compared. Substructure in the trough of the silicate band for two sources is attributed to CH3OH and NH3 in the ices, present at the similar to 2% and similar to 5% levels, respectively, relative to H2O-ice. The correlation of the silicate feature with the E(J-K) color excess is found to follow a much shallower slope relative to lines of sight that probe diffuse clouds, supporting the previous results by Chiar et al.
C1 [Chiar, J. E.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94035 USA.
[Pendleton, Y. J.; Allamandola, L. J.; Ennico, K.; Greene, T. P.; Roellig, T. L.; Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Boogert, A. C. A.] CALTECH, IPAC, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Geballe, T. R.; Mason, R. E.] No Operat Ctr, Gemini Observ, Hilo, HI 96720 USA.
[Keane, J. V.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Tielens, A. G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Whittet, D. C. B.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA.
[Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Eriksson, K.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
RP Chiar, JE (reprint author), Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave, Mountain View, CA 94035 USA.
EM jchiar@seti.org
RI Ennico, Kimberly/L-9606-2014;
OI Whittet, Douglas/0000-0001-8539-3891
FU NASA [NNX07AK38G]; NASA's Astrobiology [811073.02.12.03]; Laboratory
Astrophysics [09-APRA09-0019]; NASA Astrobiology Institute [NNA09DA80A];
Gemini Observatory; National Science Foundation
FX This work is based (in part) on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Support
for this work was provided to J.E.C. by NASA through an award issued by
JPL/Caltech and to Y.J.P., L.J.A., K. E., T. P. G., T. L. R., and S. A.
S. by NASA. L.J.A. gratefully acknowledges support from NASA's
Astrobiology (grant 811073.02.12.03) and Laboratory Astrophysics (grant
09-APRA09-0019) programs. D. C. B. W. is grateful to the NASA Exobiology
and Evolutionary Biology Program (grant NNX07AK38G) and the NASA
Astrobiology Institute (grant NNA09DA80A) for financial support. R. E.
M. and T. R. G. are supported by the Gemini Observatory, which is
operated by the Association of Universities for Research in Astronomy,
Inc., on behalf of the international Gemini partnership of Argentina,
Australia, Brazil, Canada, Chile, the United Kingdom, and the United
States of America. The work is also based in part on observations made
at the Infrared Telescope Facility, which is operated by the University
of Hawaii under Cooperative Agreement no. NCC 5-538 with the National
Aeronautics and Space Administration, Science Mission Directorate, and
Planetary Astronomy Program. 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.
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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 APR 10
PY 2011
VL 731
IS 1
AR 9
DI 10.1088/0004-637X/731/1/9
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800009
ER
PT J
AU Cowan, NB
Robinson, T
Livengood, TA
Deming, D
Agol, E
A'Hearn, MF
Charbonneau, D
Lisse, CM
Meadows, VS
Seager, S
Shields, AL
Wellnitz, DD
AF Cowan, Nicolas B.
Robinson, Tyler
Livengood, Timothy A.
Deming, Drake
Agol, Eric
A'Hearn, Michael F.
Charbonneau, David
Lisse, Carey M.
Meadows, Victoria S.
Seager, Sara
Shields, Aomawa L.
Wellnitz, Dennis D.
TI ROTATIONAL VARIABILITY OF EARTH'S POLAR REGIONS: IMPLICATIONS FOR
DETECTING SNOWBALL PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: analytical; methods: numerical; methods: observational; planets
and satellites: individual (Earth); techniques: photometric
ID GENERAL-CIRCULATION MODEL; EXTRASOLAR PLANETS; LIGHT-CURVES; PHOTOMETRIC
VARIABILITY; EXOPLANETS; ALBEDO; OCEAN; SPECTRUM; CLIMATE; SURFACE
AB We have obtained the first time-resolved, disk-integrated observations of Earth's poles with the Deep Impact spacecraft as part of the EPOXI mission of opportunity. These data mimic what we will see when we point next-generation space telescopes at nearby exoplanets. We use principal component analysis (PCA) and rotational light curve inversion to characterize color inhomogeneities and map their spatial distribution from these unusual vantage points, as a complement to the equatorial views presented by Cowan et al. in 2009. We also perform the same PCA on a suite of simulated rotational multi-band light curves from NASA's Virtual Planetary Laboratory three-dimensional spectral Earth model. This numerical experiment allows us to understand what sorts of surface features PCA can robustly identify. We find that the EPOXI polar observations have similar broadband colors as the equatorial Earth, but with 20%-30% greater apparent albedo. This is because the polar observations are most sensitive to mid-latitudes, which tend to be more cloudy than the equatorial latitudes emphasized by the original EPOXI Earth observations. The cloudiness of the mid-latitudes also manifests itself in the form of increased variability at short wavelengths in the polar observations and as a dominant gray eigencolor in the south polar observation. We construct a simple reflectance model for a snowball Earth. By construction, our model has a higher Bond albedo than the modern Earth; its surface albedo is so high that Rayleigh scattering does not noticeably affect its spectrum. The rotational color variations occur at short wavelengths due to the large contrast between glacier ice and bare land in those wavebands. Thus, we find that both the broadband colors and diurnal color variations of such a planet would be easily distinguishable from the modern-day Earth, regardless of viewing angle.
C1 [Cowan, Nicolas B.] Northwestern Univ, Evanston, IL 60208 USA.
[Robinson, Tyler; Agol, Eric; Meadows, Victoria S.; Shields, Aomawa L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Robinson, Tyler; Agol, Eric; Meadows, Victoria S.; Shields, Aomawa L.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Livengood, Timothy A.; Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[A'Hearn, Michael F.; Wellnitz, Dennis D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, Cambridge, MA 02139 USA.
RP Cowan, NB (reprint author), Northwestern Univ, 2131 Tech Dr, Evanston, IL 60208 USA.
EM n-cowan@northwestern.edu
RI Wellnitz, Dennis/B-4080-2012; Livengood, Timothy/C-8512-2012; Agol,
Eric/B-8775-2013; Lisse, Carey/B-7772-2016;
OI Agol, Eric/0000-0002-0802-9145; Lisse, Carey/0000-0002-9548-1526;
Charbonneau, David/0000-0002-9003-484X
FU NASA; National Science Foundation
FX This work was supported by the NASA Discovery Program. We thank D. S.
Abbot and R. T. Pierrehumbert for providing us with cloud maps of
snowball Earth. N.B.C. acknowledges many useful discussions with S. G.
Warren about snowball Earth, and thanks W. Sullivan for encouraging him
to complete his astrobiology research rotation. E.A. is supported by a
National Science Foundation Career Grant.
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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 APR 10
PY 2011
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DI 10.1088/0004-637X/731/1/76
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800076
ER
PT J
AU Hong, S
Calzetti, D
Dopita, MA
Blair, WP
Whitmore, BC
Balick, B
Bond, HE
Carollo, M
Disney, MJ
Frogel, JA
Hall, D
Holtzman, JA
Kimble, RA
McCarthy, PJ
O'Connell, RW
Paresce, F
Saha, A
Silk, JI
Trauger, JT
Walker, AR
Windhorst, RA
Young, ET
Mutchler, M
AF Hong, Sungryong
Calzetti, Daniela
Dopita, Michael A.
Blair, William P.
Whitmore, Bradley C.
Balick, Bruce
Bond, Howard E.
Carollo, Marcella
Disney, Michael J.
Frogel, Jay A.
Hall, Donald
Holtzman, Jon A.
Kimble, Randy A.
McCarthy, Patrick J.
O'Connell, Robert W.
Paresce, Francesco
Saha, Abhijit
Silk, Joseph I.
Trauger, John T.
Walker, Alistair R.
Windhorst, Rogier A.
Young, Erick T.
Mutchler, Max
TI LARGE-SCALE SHOCK-IONIZED AND PHOTOIONIZED GAS IN M83: THE IMPACT OF
STAR FORMATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: interactions; galaxies: ISM; galaxies: starburst; ISM:
structure
ID HUBBLE-SPACE-TELESCOPE; II ESI SPECTRA; FIELD CAMERA 3; STARBURST
GALAXIES; HII-REGIONS; INTERSTELLAR-MEDIUM; GASEOUS OUTFLOWS; YOUNG
CLUSTERS; MODELS; SPECTROSCOPY
AB We investigate the ionization structure of the nebular gas in M83 using the line diagnostic diagram, [O III](5007 angstrom)/H beta versus [S II](6716 angstrom+6731 angstrom)/H alpha, with the newly available narrowband images from the Wide Field Camera 3 (WFC3) of the Hubble Space Telescope (HST). We produce the diagnostic diagram on a pixel-by-pixel (0 ''.2 x 0 ''.2) basis and compare it with several photo- and shock-ionization models. We select four regions from the center to the outer spiral arm and compare them in the diagnostic diagram. For the photoionized gas, we observe a gradual increase of the log ([O III]/H beta) ratios from the center to the spiral arm, consistent with the metallicity gradient, as the H II regions go from super-solar abundance to roughly solar abundance from the center out. Using the diagnostic diagram, we separate the photoionized from the shock-ionized component of the gas. We find that the shock-ionized H alpha emission ranges from similar to 2% to about 15%-33% of the total, depending on the separation criteria used. An interesting feature in the diagnostic diagram is a horizontal distribution around log ([O III]/H beta) approximate to 0. This feature is well fit by a shock-ionization model with 2.0 Z(circle dot) metallicity and shock velocities in the range of 250350 km s(-1). A low-velocity shock component, <200 km s(-1), is also detected and is spatially located at the boundary between the outer ring and the spiral arm. The low-velocity shock component can be due to (1) supernova remnants located nearby, (2) dynamical interaction between the outer ring and the spiral arm, and (3) abnormal line ratios from extreme local dust extinction. The current data do not enable us to distinguish among those three possible interpretations. Our main conclusion is that, even at the HST resolution, the shocked gas represents a small fraction of the total ionized gas emission at less than 33% of the total. However, it accounts for virtually all of the mechanical energy produced by the central starburst in M83.
C1 [Hong, Sungryong; Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Whitmore, Bradley C.; Bond, Howard E.; Mutchler, Max] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Carollo, Marcella] ETH, Dept Phys, CH-8093 Zurich, Switzerland.
[Disney, Michael J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Frogel, Jay A.] Assoc Univ Res Astron, Washington, DC 20005 USA.
[Hall, Donald] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCarthy, Patrick J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Paresce, Francesco] INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy.
[Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Silk, Joseph I.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Trauger, John T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walker, Alistair R.] Cerro Tololo Interamer Observ, La Serena, Chile.
[Windhorst, Rogier A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Young, Erick T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Hong, S (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
EM wpb@pha.jhu.edu
RI Dopita, Michael/P-5413-2014;
OI Dopita, Michael/0000-0003-0922-4986; silk, joe/0000-0002-1566-8148
FU NASA [NAS5-26555]
FX We are grateful to an anonymous referee for comments that have improved
this paper. This paper is based on observations taken with the NASA/ESA
Hubble Space Telescope obtained at the Space Telescope Science
Institute, which is operated by AURA, Inc., under NASA contract
NAS5-26555. It uses Early Release Science observations made by the WFC3
Science Oversight Committee. We are grateful to the Director of STScI
for awarding Director's Discretionary Time for this program.
NR 40
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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 APR 10
PY 2011
VL 731
IS 1
AR 45
DI 10.1088/0004-637X/731/1/45
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800045
ER
PT J
AU Jia, JJ
Ptak, A
Heckman, TM
Overzier, RA
Hornschemeier, A
LaMassa, SM
AF Jia, Jianjun
Ptak, Andrew
Heckman, Timothy M.
Overzier, Roderik A.
Hornschemeier, Ann
LaMassa, Stephanie M.
TI EVIDENCE FOR BLACK HOLE GROWTH IN LOCAL ANALOGS TO LYMAN BREAK GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: starburst; quasars: general; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATE; ULTRALUMINOUS INFRARED
GALAXIES; ULTRAVIOLET-LUMINOUS GALAXIES; TYPE-2 SEYFERT-GALAXIES; X-RAY
OBSERVATIONS; PARAMETER-ESTIMATION; INTERSTELLAR-MEDIUM; FORMING
GALAXIES; FAR-ULTRAVIOLET
AB We have used XMM-Newton to observe six Lyman break analogs (LBAs): members of the rare population of local galaxies that have properties that are very similar to distant Lyman break galaxies. Our six targets were specifically selected because they have optical emission-line properties that are intermediate between starbursts and Type 2 (obscured) active galactic nuclei (AGNs). Our new X-ray data provide an important diagnostic of the presence of an AGN. We find X-ray luminosities of order 10(42) erg s(-1) and ratios of X-ray to far-IR luminosities that are higher than values in pure starburst galaxies by factors ranging from similar to 3 to 30. This strongly suggests the presence of an AGN in at least some of the galaxies. The ratios of the luminosities of the hard (2-10 keV) X-ray to [O III]lambda 5007 emission line are low by about an order of magnitude compared with Type 1 AGN, but are consistent with the broad range seen in Type 2 AGN. Either the AGN hard X-rays are significantly obscured or the [O III] emission is dominated by the starburst. We searched for an iron emission line at similar to 6.4 keV, which is a key feature of obscured AGNs, but only detected emission at the similar to 2 sigma level. Finally, we find that the ratios of the mid-infrared (24 mu m) continuum to [O III]lambda 5007 luminosities in these LBAs are higher than the values for Type 2 AGN by an average of 0.8 dex. Combining all these clues, we conclude that an AGN is likely to be present, but that the bolometric luminosity is produced primarily by an intense starburst. If these black holes are radiating at the Eddington limit, their masses would lie in the range of 10(5)-10(6) M circle dot. These objects may offer ideal local laboratories to investigate the processes by which black holes grew in the early universe.
C1 [Jia, Jianjun; Heckman, Timothy M.; LaMassa, Stephanie M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ptak, Andrew; Hornschemeier, Ann] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Overzier, Roderik A.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
RP Jia, JJ (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
FU NASA [NNX08AZ0G]
FX We are very grateful to the anonymous referee for helpful comments that
have improved the manuscript. We also thank Marat Gilfanov for
discussion. This work is supported by NASA grant NNX08AZ0G.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2011
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PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800055
ER
PT J
AU Krughoff, KS
Connolly, AJ
Frieman, J
SubbaRao, M
Kilper, G
Schneider, DP
AF Krughoff, K. Simon
Connolly, Andrew J.
Frieman, Joshua
SubbaRao, Mark
Kilper, Gary
Schneider, Donald P.
TI SPECTROSCOPIC DETERMINATION OF THE LOW-REDSHIFT TYPE Ia SUPERNOVA RATE
FROM THE SLOAN DIGITAL SKY SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; supernovae: general; techniques: spectroscopic
ID DELAY-TIME DISTRIBUTION; SURVEY IMAGING DATA; STAR-FORMATION; DATA
RELEASE; SPECTRAL CLASSIFICATION; ULTRAVIOLET EXTINCTION; LEGACY SURVEY;
LIGHT CURVES; DEEP SURVEY; PROGENITORS
AB Supernova rates (SNRs) are directly coupled to high-mass stellar birth and evolution. As such, they are one of the few direct measures of the history of cosmic stellar evolution. In this paper, we describe a probabilistic technique for identifying supernovae within spectroscopic samples of galaxies. We present a study of 52 Type Ia supernovae ranging in age from -14 days to +40 days extracted from a parent sample of similar to 350,000 spectra from the SDSS DR5. We find an SNR of 0.472(-0.039)(+0.048) (Systematic)(-0.071)(+0.081)(Statistical)SNu at a redshift of < z > = 0.1. This value is higher than other values at low redshift at the 1 sigma level, but is consistent at the 3 sigma level. In this paper, we demonstrate the potential for the described approach to detect supernovae in future spectroscopic surveys.
C1 [Krughoff, K. Simon; Connolly, Andrew J.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Frieman, Joshua] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Frieman, Joshua] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Frieman, Joshua; SubbaRao, Mark] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[SubbaRao, Mark] Adler Planetarium & Astron Museum, Chicago, IL 60605 USA.
[Kilper, Gary] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 408A, University Pk, PA 16802 USA.
RP Krughoff, KS (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
FU NSF [AST-0851007]; DOE [DE-FG02-87ER40315]; Alfred P. Sloan Foundation;
National Science Foundation; U.S. Department of Energy; National
Aeronautics and Space Administration; Japanese Monbukagakusho; Max
Planck Society; Higher Education Funding Council for England; American
Museum of Natural History; Astrophysical Institute Potsdam,; University
of Basel; University of Cambridge; Case Western Reserve University;
University of Chicago; Drexel University; Fermilab; Institute for
Advanced Study; Japan Participation Group; Johns Hopkins University;
Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle
Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of
Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute
for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New
Mexico State University; Ohio State University; University of
Pittsburgh; University of Portsmouth; Princeton University; United
States Naval Observatory; University of Washington
FX The authors wish to thank the reviewer for many excellent points that
served to greatly improve the quality of the analysis. K. S. K. and
A.J.C. acknowledge partial support from NSF grant AST-0851007 and DOE
grant DE-FG02-87ER40315. 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2011
VL 731
IS 1
AR 42
DI 10.1088/0004-637X/731/1/42
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800042
ER
PT J
AU Mainzer, A
Bauer, J
Grav, T
Masiero, J
Cutri, RM
Dailey, J
Eisenhardt, P
McMillan, RS
Wright, E
Walker, R
Jedicke, R
Spahr, T
Tholen, D
Alles, R
Beck, R
Brandenburg, H
Conrow, T
Evans, T
Fowler, J
Jarrett, T
Marsh, K
Masci, F
McCallon, H
Wheelock, S
Wittman, M
Wyatt, P
DeBaun, E
Elliott, G
Elsbury, D
Gautier, T
Gomillion, S
Leisawitz, D
Maleszewski, C
Micheli, M
Wilkins, A
AF Mainzer, A.
Bauer, J.
Grav, T.
Masiero, J.
Cutri, R. M.
Dailey, J.
Eisenhardt, P.
McMillan, R. S.
Wright, E.
Walker, R.
Jedicke, R.
Spahr, T.
Tholen, D.
Alles, R.
Beck, R.
Brandenburg, H.
Conrow, T.
Evans, T.
Fowler, J.
Jarrett, T.
Marsh, K.
Masci, F.
McCallon, H.
Wheelock, S.
Wittman, M.
Wyatt, P.
DeBaun, E.
Elliott, G.
Elsbury, D.
Gautier, T.
Gomillion, S.
Leisawitz, D.
Maleszewski, C.
Micheli, M.
Wilkins, A.
TI PRELIMINARY RESULTS FROM NEOWISE: AN ENHANCEMENT TO THE WIDE-FIELD
INFRARED SURVEY EXPLORER FOR SOLAR SYSTEM SCIENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; comets: general; minor planets, asteroids: general; surveys
ID NEAR-EARTH ASTEROIDS; JOVIAN TROJAN ASTEROIDS; DUST TRAILS; SIZE
DISTRIBUTIONS; PERIOD COMETS; OORT CLOUD; ORIGIN; MISSION; OBJECTS; IRAS
AB The Wide-field Infrared Survey Explorer (WISE) has surveyed the entire sky at four infrared wavelengths with greatly improved sensitivity and spatial resolution compared to its predecessors, the Infrared Astronomical Satellite and the Cosmic Background Explorer. NASA's Planetary Science Division has funded an enhancement to the WISE data processing system called "NEOWISE" that allows detection and archiving of moving objects found in the WISE data. NEOWISE has mined the WISE images for a wide array of small bodies in our solar system, including near-Earth objects (NEOs), Main Belt asteroids, comets, Trojans, and Centaurs. By the end of survey operations in 2011 February, NEOWISE identified over 157,000 asteroids, including more than 500 NEOs and similar to 120 comets. The NEOWISE data set will enable a panoply of new scientific investigations.
C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J.; Cutri, R. M.; Dailey, J.; Alles, R.; Beck, R.; Brandenburg, H.; Conrow, T.; Evans, T.; Fowler, J.; Jarrett, T.; Marsh, K.; Masci, F.; McCallon, H.; Wheelock, S.; Wittman, M.; Wyatt, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Grav, T.] Johns Hopkins Univ, Dept Astron, Baltimore, MD USA.
[McMillan, R. S.; Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Wright, E.] UCLA Astron, Los Angeles, CA 90095 USA.
[Walker, R.] Monterey Inst Res Astron, Monterey, CA USA.
[Jedicke, R.; Tholen, D.; Elliott, G.; Micheli, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[DeBaun, E.] Dartmouth Coll, Hanover, NH 03755 USA.
[Elsbury, D.] Notre Dame High Sch, Sherman Oaks, CA 91423 USA.
[Gautier, T.] Flintridge Preparatory Sch, La Canada Flintridge, CA 91101 USA.
[Gomillion, S.] Embry Riddle Aeronaut Univ, Daytona Beach, FL 32114 USA.
[Leisawitz, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM amainzer@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X; Micheli, Marco/0000-0001-7895-8209
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 WISE, 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
Union's Minor Planet Center, operated by the Harvard-Smithsonian Center
for Astrophysics, and the Central Bureau for Astronomical Telegrams,
operated by Harvard University. We appreciate the contributions of the
referee, J. Emery, which greatly improved the manuscript. 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. We thank the Auton Lab of Carnegie Mellon University for
use of their libraries, and the PanSTARRS project for MOPS.
NR 80
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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 APR 10
PY 2011
VL 731
IS 1
AR 53
DI 10.1088/0004-637X/731/1/53
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800053
ER
PT J
AU Schwadron, NA
Allegrini, F
Bzowski, M
Christian, ER
Crew, GB
Dayeh, M
DeMajistre, R
Frisch, P
Funsten, HO
Fuselier, SA
Goodrich, K
Gruntman, M
Janzen, P
Kucharek, H
Livadiotis, G
McComas, DJ
Moebius, E
Prested, C
Reisenfeld, D
Reno, M
Roelof, E
Siegel, J
Vanderspek, R
AF Schwadron, N. A.
Allegrini, F.
Bzowski, M.
Christian, E. R.
Crew, G. B.
Dayeh, M.
DeMajistre, R.
Frisch, P.
Funsten, H. O.
Fuselier, S. A.
Goodrich, K.
Gruntman, M.
Janzen, P.
Kucharek, H.
Livadiotis, G.
McComas, D. J.
Moebius, E.
Prested, C.
Reisenfeld, D.
Reno, M.
Roelof, E.
Siegel, J.
Vanderspek, R.
TI SEPARATION OF THE INTERSTELLAR BOUNDARY EXPLORER RIBBON FROM GLOBALLY
DISTRIBUTED ENERGETIC NEUTRAL ATOM FLUX
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: general; magnetohydrodynamics (MHD); plasmas; shock waves; solar
wind; Sun: heliosphere
ID SOLAR-WIND; TERMINATION SHOCK; MAGNETIC-FIELD; OUTER HELIOSPHERE; IBEX
RIBBON; PICKUP IONS; ENA FLUX; HELIOSHEATH; MECHANISM; GENERATION
AB The Interstellar Boundary Explorer (IBEX) observes a remarkable feature, the IBEX ribbon, which has energetic neutral atom (ENA) flux over a narrow region similar to 20 degrees. wide, a factor of 2-3 higher than the more globally distributed ENA flux. Here, we separate ENA emissions in the ribbon from the distributed flux by applying a transparency mask over the ribbon and regions of high emissions, and then solve for the distributed flux using an interpolation scheme. Our analysis shows that the energy spectrum and spatial distribution of the ribbon are distinct from the surrounding globally distributed flux. The ribbon energy spectrum shows a knee between similar to 1 and 4 keV, and the angular distribution is approximately independent of energy. In contrast, the distributed flux does not show a clear knee and more closely conforms to a power law over much of the sky. Consistent with previous analyses, the slope of the power law steepens from the nose to tail, suggesting a weaker termination shock toward the tail as compared to the nose. The knee in the energy spectrum of the ribbon suggests that its source plasma population is generated via a distinct physical process. Both the slope in the energy distribution of the distributed flux and the knee in the energy distribution of the ribbon are ordered by latitude. The heliotail may be identified in maps of globally distributed flux as a broad region of low flux centered similar to 44 degrees W of the interstellar downwind direction, suggesting heliotail deflection by the interstellar magnetic field.
C1 [Schwadron, N. A.; Kucharek, H.; Moebius, E.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Schwadron, N. A.; Allegrini, F.; Dayeh, M.; Livadiotis, G.; McComas, D. J.; Reno, M.] SW Res Inst, San Antonio, TX 78228 USA.
[Allegrini, F.; McComas, D. J.] Univ Texas San Antonio, Dept Phys, San Antonio, TX 78249 USA.
[Bzowski, M.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland.
[Christian, E. R.; Vanderspek, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Crew, G. B.; Roelof, E.] MIT, Cambridge, MA 02139 USA.
[DeMajistre, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Frisch, P.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Funsten, H. O.; Goodrich, K.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Fuselier, S. A.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA.
[Gruntman, M.] Univ So Calif, Dept Astronaut Engn, Los Angeles, CA 90089 USA.
[Janzen, P.; Reisenfeld, D.] Univ Montana, Dept Phys, Missoula, MT 59812 USA.
[Prested, C.; Siegel, J.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
RP Schwadron, NA (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
EM n.schwadron@unh.edu; fallegrini@swri.edu; bzowski@cbk.waw.pl;
eric.r.christian@nasa.gov; gbc@space.mit.edu; maldayeh@swri.edu;
Bob.DeMajistre@jhuapl.edu; frisch@oddjob.uchicago.edu;
hfunsten@lanl.gov; stephen.a.fuselier@lmco.com; kgoodri@lanl.gov;
mikeg@usc.edu; paul.janzen@umontana.edu; harald.kucharek@unh.edu;
george.livadiotis@swri.org; dmccomas@swri.org; eberhard.moebius@unh.edu;
cprested@bu.edu; dan.reisenfeld@umontana.edu; mreno@swri.edu;
Edmond.Roelof@jhuapl.edu; jacob707@gmail.com
RI Christian, Eric/D-4974-2012; Funsten, Herbert/A-5702-2015; Reisenfeld,
Daniel/F-7614-2015; Gruntman, Mike/A-5426-2008;
OI Christian, Eric/0000-0003-2134-3937; Funsten,
Herbert/0000-0002-6817-1039; Gruntman, Mike/0000-0002-0830-010X;
Moebius, Eberhard/0000-0002-2745-6978
FU NASA; Polish Ministry for Science and Higher Education [NS-1260-11-09]
FX We are deeply indebted to all of the outstanding people who have made
the IBEX mission possible. This work was carried out as a part of the
IBEX project, with support from NASA's Explorer Program and Polish
Ministry for Science and Higher Education (grant NS-1260-11-09).
NR 40
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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 APR 10
PY 2011
VL 731
IS 1
AR 56
DI 10.1088/0004-637X/731/1/56
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800056
ER
PT J
AU Spezzi, L
Beccari, G
De Marchi, G
Young, ET
Paresce, F
Dopita, MA
Andersen, M
Panagia, N
Balick, B
Bond, HE
Calzetti, D
Carollo, CM
Disney, MJ
Frogel, JA
Hall, DNB
Holtzman, JA
Kimble, RA
McCarthy, PJ
O'Connell, RW
Ryan, RE
Saha, A
Silk, JI
Trauger, JT
Walker, AR
Whitmore, BC
Windhorst, RA
AF Spezzi, Loredana
Beccari, Giacomo
De Marchi, Guido
Young, Erick T.
Paresce, Francesco
Dopita, Michael A.
Andersen, Morten
Panagia, Nino
Balick, Bruce
Bond, Howard E.
Calzetti, Daniela
Carollo, C. Marcella
Disney, Michael J.
Frogel, Jay A.
Hall, Donald N. B.
Holtzman, Jon A.
Kimble, Randy A.
McCarthy, Patrick J.
O'Connell, Robert W.
Ryan, Russell E., Jr.
Saha, Abhijit
Silk, Joseph I.
Trauger, John T.
Walker, Alistair R.
Whitmore, Bradley C.
Windhorst, Rogier A.
TI DETECTION OF BROWN DWARF LIKE OBJECTS IN THE CORE OF NGC 3603
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; instrumentation: photometers; open clusters and
associations: individual (NCG 3603); stars: pre-main sequence;
techniques: photometric
ID INITIAL MASS FUNCTION; NEAR-INFRARED SPECTRA; STAR-FORMING REGION; GIANT
BRANCH STARS; EVOLUTIONARY MODELS; ORBITAL PERIOD; TAURUS-AURIGA; YOUNG
CLUSTER; HII-REGIONS; SKY SURVEY
AB We used near-infrared data obtained with the Wide Field Camera 3 on the Hubble Space Telescope to identify objects having the colors of brown dwarfs (BDs) in the field of the massive galactic cluster NGC 3603. These are identified through a combination of narrow-and medium-band filters which span the J and H bands and are particularly sensitive to the presence of the 1.3-1.5 mu m H2O molecular band unique to BDs. We provide a calibration of the relationship between effective temperature and color for both field stars and BDs. This photometric method provides effective temperatures for BDs to an accuracy of +/-350K relative to spectroscopic techniques. This accuracy is shown to be not significantly affected by either stellar surface gravity or uncertainties in the interstellar extinction. We identify nine objects having effective temperatures between 1700 and 2200 K, typical of BDs, observed J-band magnitudes in the range 19.5-21.5, and that are strongly clustered toward the luminous core of NGC 3603. However, if these are located at the distance of the cluster, they are far too luminous to be normal BDs. We argue that it is unlikely that these objects are either artifacts of our data set, normal field BDs/M-type giants, or extragalactic contaminants and, therefore, might represent a new class of stars having the effective temperatures of BDs but with luminosities of more massive stars. We explore the interesting scenario in which these objects would be normal stars that have recently tidally ingested a hot Jupiter, the remnants of which are providing a short-lived extended photosphere to the central star. In this case, we would expect them to show the signature of fast rotation.
C1 [Spezzi, Loredana; Beccari, Giacomo; De Marchi, Guido; Andersen, Morten] European Space Agcy ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Young, Erick T.] NASA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Paresce, Francesco] Ist Fis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy.
[Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Panagia, Nino; Bond, Howard E.; Whitmore, Bradley C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Carollo, C. Marcella] ETH, Dept Phys, CH-8093 Zurich, Switzerland.
[Disney, Michael J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Frogel, Jay A.] Assoc Univ Res Astron, Washington, DC 20005 USA.
[Hall, Donald N. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCarthy, Patrick J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Ryan, Russell E., Jr.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Silk, Joseph I.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Trauger, John T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walker, Alistair R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile.
[Windhorst, Rogier A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Spezzi, L (reprint author), European Space Agcy ESTEC, POB 299, NL-2200 AG Noordwijk, Netherlands.
EM lspezzi@rssd.esa.int
RI Dopita, Michael/P-5413-2014;
OI Dopita, Michael/0000-0003-0922-4986; silk, joe/0000-0002-1566-8148
FU Australian Research Council (ARC) [DP0984657, DP0664434]
FX This paper is based on Early Release Science observations made by the
WFC3 Scientific Oversight Committee. We are grateful to the Director of
the Space Telescope Science Institute for awarding Director's
Discretionary Time for this program. We thank B. Burningham for
providing unpublished spectra of brown dwarfs, X. Pang and A. Pasquali
for providing unpublished information on reddening effects in NGC 3603,
and the anonymous referee for his careful reading and useful
comments/suggestions. M. A. D. acknowledges the support of the
Australian Research Council (ARC) through Discovery projects DP0984657
and DP0664434. We also acknowledge extensive use of the SIMBAD database,
operated at CDS Strasbourg, the SpeX Prism Spectral Libraries,
maintained by A. Burgasser, and the Multimission Archive at the Space
Telescope Science Institute.
NR 87
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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 APR 10
PY 2011
VL 731
IS 1
AR 1
DI 10.1088/0004-637X/731/1/1
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 753KR
UT WOS:000289772800001
ER
PT J
AU Zhu, L
Martins, JV
Remer, LA
AF Zhu, L.
Martins, J. V.
Remer, L. A.
TI Biomass burning aerosol absorption measurements with MODIS using the
critical reflectance method
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID REMOTE-SENSING OBSERVATIONS; BLACK CARBON AEROSOLS; MINERAL DUST TYPES;
LIGHT-ABSORPTION; HYDROLOGICAL CYCLE; OPTICAL-PROPERTIES; SOUTHERN
AFRICA; SKY RADIANCE; CLIMATE; SATELLITE
AB This research uses the critical reflectance technique, a space-based remote sensing method, to measure the spatial distribution of aerosol absorption properties over land. Choosing two regions dominated by biomass burning aerosols, a series of sensitivity studies were undertaken to analyze the potential limitations of this method for the type of aerosol to be encountered in the selected study areas, and to show that the retrieved results are relatively insensitive to uncertainties in the assumptions used in the retrieval of smoke aerosol. The critical reflectance technique is then applied to Moderate Resolution Imaging Spectrometer (MODIS) data to retrieve the spectral aerosol single-scattering albedo (SSA) in South African and South American biomass burning events. The retrieved results were validated with collocated Aerosol Robotic Network (AERONET) retrievals. Approximately 67% of the comparisons show a difference between MODIS and AERONET smaller than 0.03, the magnitude of the AERONET uncertainty. The overlap of the two retrievals increases to 88%, allowing for measurement variance in the MODIS retrievals, as well. The ensemble average of MODIS-derived SSA for the Amazon forest station is 0.92 at 670 nm, and 0.84-0.89 for the southern African savanna stations. The critical reflectance technique allows evaluation of the spatial variability of SSA and shows that SSA in South America exhibits higher spatial variation than in South Africa. The accuracy of the retrieved aerosol SSA from MODIS data indicates that this product can help to better understand how aerosols affect the regional and global climate.
C1 [Zhu, L.; Martins, J. V.] Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Remer, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhu, L (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Earth Syst Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM zhuli1@umbc.edu; martins@umbc.edu; Lorraine.A.Remer@nasa.gov
FU NASA [NNX08AJ78G]
FX We would like to thank NASA for funding this project under grant
NNX08AJ78G. We also would like to thank the MODIS and AERONET teams for
their excellent work on the instrument development, maintenance, and
calibration. We thank their effort on data quality control and for
providing data to the public, as well. Thanks also go to Kelley Wells,
Alexandre Correia, Tom Eck, Tianle Yuan, Ralph Kahn, and the anonymous
reviewers for their constructive comments and suggestions.
NR 54
TC 12
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U1 0
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 APR 9
PY 2011
VL 116
AR D07202
DI 10.1029/2010JD015187
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 747ZO
UT WOS:000289360000002
ER
PT J
AU Kramer, GY
Besse, S
Nettles, J
Combe, JP
Clark, RN
Pieters, CM
Staid, M
Malaret, E
Boardman, J
Green, RO
Head, JW
McCord, TB
AF Kramer, Georgiana Y.
Besse, Sebastien
Nettles, Jeffrey
Combe, Jean-Philippe
Clark, Roger N.
Pieters, Carle M.
Staid, Matthew
Malaret, Erik
Boardman, Joseph
Green, Robert O.
Head, James W., III
McCord, Thomas B.
TI Newer views of the Moon: Comparing spectra from Clementine and the Moon
Mineralogy Mapper
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ABSOLUTE CALIBRATION; MARE SOILS; REFLECTANCE; TRANSPORT; CRATERS;
SURFACE
AB The Moon Mineralogy Mapper (M-3) provided the first global hyperspectral data of the lunar surface in 85 bands from 460 to 2980 nm. The Clementine mission provided the first global multispectral maps the lunar surface in 11 spectral bands across the ultraviolet-visible (UV-VIS) and near-infrared (NIR). In an effort to understand how M-3 improves our ability to analyze and interpret lunar data, we compare M-3 spectra with those from Clementine's UV-VIS and NIR cameras. The Clementine mission provided the first global multispectral maps the lunar surface in 11 spectral bands across the UV-VIS and NIR. We have found that M-3 reflectance values are lower across all wavelengths compared with albedos from both of Clementine's UV-VIS and NIR cameras. M-3 spectra show the Moon to be redder, that is, have a steeper continuum slope, than indicated by Clementine. The 1 mu m absorption band depths may be comparable between the instruments, but Clementine data consistently exhibit shallower 2 mu m band depths than M-3. Absorption band minimums are difficult to compare due to the significantly different spectral resolutions.
C1 [Kramer, Georgiana Y.; Combe, Jean-Philippe; McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Besse, Sebastien] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Nettles, Jeffrey; Pieters, Carle M.; Head, James W., III] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Clark, Roger N.] US Geol Survey, Fed Ctr, Denver, CO 80225 USA.
[Staid, Matthew] Planetary Sci Inst, Napa Valley, CA USA.
[Malaret, Erik] Appl Coherent Technol, Herndon, VA 20170 USA.
[Boardman, Joseph] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA.
[Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kramer, GY (reprint author), Bear Fight Inst, 22 Fiddlers Rd,Box 667, Winthrop, WA 98862 USA.
EM kramer@lpi.usra.edu
OI Besse, Sebastien/0000-0002-1052-5439
NR 34
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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-PLANET
JI J. Geophys. Res.-Planets
PD APR 9
PY 2011
VL 116
AR E00G04
DI 10.1029/2010JE003728
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 748AD
UT WOS:000289361500001
ER
PT J
AU Xu, LA
Samanta, A
Costa, MH
Ganguly, S
Nemani, RR
Myneni, RB
AF Xu, Liang
Samanta, Arindam
Costa, Marcos H.
Ganguly, Sangram
Nemani, Ramakrishna R.
Myneni, Ranga B.
TI Widespread decline in greenness of Amazonian vegetation due to the 2010
drought
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID RAIN-FORESTS; CLIMATE; INFORMATION; SATELLITE; BIOMASS; DIEBACK;
INDEXES; GROWTH; MODEL
AB During this decade, the Amazon region has suffered two severe droughts in the short span of five years - 2005 and 2010. Studies on the 2005 drought present a complex, and sometimes contradictory, picture of how these forests have responded to the drought. Now, on the heels of the 2005 drought, comes an even stronger drought in 2010, as indicated by record low river levels in the 109 years of bookkeeping. How has the vegetation in this region responded to this record-breaking drought? Here we report widespread, severe and persistent declines in vegetation greenness, a proxy for photosynthetic carbon fixation, in the Amazon region during the 2010 drought based on analysis of satellite measurements. The 2010 drought, as measured by rainfall deficit, affected an area 1.65 times larger than the 2005 drought - nearly 5 million km(2) of vegetated area in Amazonia. The decline in greenness during the 2010 drought spanned an area that was four times greater (2.4 million km(2)) and more severe than in 2005. Notably, 51% of all drought-stricken forests showed greenness declines in 2010 (1.68 million km(2)) compared to only 14% in 2005 (0.32 million km(2)). These declines in 2010 persisted following the end of the dry season drought and return of rainfall to normal levels, unlike in 2005. Overall, the widespread loss of photosynthetic capacity of Amazonian vegetation due to the 2010 drought may represent a significant perturbation to the global carbon cycle. Citation: Xu, L., A. Samanta, M. H. Costa, S. Ganguly, R. R. Nemani, and R. B. Myneni (2011), Widespread decline in greenness of Amazonian vegetation due to the 2010 drought, Geophys. Res. Lett., 38, L07402, doi:10.1029/2011GL046824.
C1 [Xu, Liang; Samanta, Arindam; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Samanta, Arindam] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
[Costa, Marcos H.] Univ Fed Vicosa, Dept Agr & Environm Engn, BR-36570000 Vicosa, MG, Brazil.
[Ganguly, Sangram] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA 94035 USA.
RP Xu, LA (reprint author), Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
EM arindam.sam@gmail.com
RI Xu, Liang/D-1247-2013; ganguly, sangram/B-5108-2010; Myneni,
Ranga/F-5129-2012
FU NASA
FX We acknowledge funding from Earth science and Advanced Information
Systems Technology programs at NASA. This research was performed using
NASA Earth Exchange. NEX combines state-of-the-art supercomputing, Earth
system modeling, remote sensing data from NASA and other agencies, and a
scientific social networking platform to deliver a complete work
environment in which users can explore and analyze large Earth science
data sets, run modeling codes, collaborate on new or existing projects,
and share results within and/or among communities. Arindam Samanta and
Liang Xu contributed equally to this work.
NR 27
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U1 2
U2 37
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 APR 8
PY 2011
VL 38
AR L07402
DI 10.1029/2011GL046824
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 747YM
UT WOS:000289357200001
ER
PT J
AU Pi, XQ
Freeman, A
Chapman, B
Rosen, P
Li, ZH
AF Pi, Xiaoqing
Freeman, Anthony
Chapman, Bruce
Rosen, Paul
Li, Zhenhong
TI Imaging ionospheric inhomogeneities using spaceborne synthetic aperture
radar
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LATITUDE; CALIBRATION
AB We present a technique and results of 2-D imaging of Faraday rotation and total electron content using spaceborne L band polarimetric synthetic aperture radar (PolSAR). The results are obtained by processing PolSAR data collected using the Phased Array type L-band Synthetic Aperture Radar (PALSAR) on board the Advanced Land Observation Satellite. Distinguished ionospheric inhomogeneities are captured in 2-D images from space with relatively high resolutions of hundreds of meters to a couple of kilometers in auroral-, middle-, and low-latitude regions. The observed phenomena include aurora-associated ionospheric enhancement arcs, the middle- latitude trough, traveling ionospheric disturbances, and plasma bubbles, as well as ionospheric irregularities. These demonstrate a new capability of spaceborne synthetic aperture radar that will not only provide measurements to correction of ionospheric effects in Earth science imagery but also significantly benefit ionospheric studies.
C1 [Pi, Xiaoqing; Freeman, Anthony; Chapman, Bruce; Rosen, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Li, Zhenhong] Univ Glasgow, Dept Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland.
RP Pi, XQ (reprint author), CALTECH, Jet Prop Lab, M-S 138-308,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM xiaoqing.pi@jpl.nasa.gov
RI NCEO, COMET+`/A-3443-2013; Li, Zhenhong/F-8705-2010
OI Li, Zhenhong/0000-0002-8054-7449
FU NASA
FX The authors thank the Japanese Aerospace and Exploration Agency, the
Earth Observation Research Center of Japan, and Masanobu Shimada for
providing PALSAR data for this study, and the Alaska Satellite Facility
for processing and distributing PALSAR data. The authors also thank the
International GNSS Service (IGS) for organizing the IGS GPS networking
and archiving, as well as distributing the GPS data that are used in
this study, and the Geographical Survey Institute of Japan and Akinori
Saito at Kyoto University for providing the GEONET GPS TEC data for this
study. The research performed at the Jet Propulsion Laboratory,
California Institute of Technology, is under a contract with NASA.
NR 24
TC 18
Z9 18
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR 8
PY 2011
VL 116
AR A04303
DI 10.1029/2010JA016267
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 747YR
UT WOS:000289357700002
ER
PT J
AU Beck, PG
Bedding, TR
Mosser, B
Stello, D
Garcia, RA
Kallinger, T
Hekker, S
Elsworth, Y
Frandsen, S
Carrier, F
De Ridder, J
Aerts, C
White, TR
Huber, D
Dupret, MA
Montalban, J
Miglio, A
Noels, A
Chaplin, WJ
Kjeldsen, H
Christensen-Dalsgaard, J
Gilliland, RL
Brown, TM
Kawaler, SD
Mathur, S
Jenkins, JM
AF Beck, P. G.
Bedding, T. R.
Mosser, B.
Stello, D.
Garcia, R. A.
Kallinger, T.
Hekker, S.
Elsworth, Y.
Frandsen, S.
Carrier, F.
De Ridder, J.
Aerts, C.
White, T. R.
Huber, D.
Dupret, M-A
Montalban, J.
Miglio, A.
Noels, A.
Chaplin, W. J.
Kjeldsen, H.
Christensen-Dalsgaard, J.
Gilliland, R. L.
Brown, T. M.
Kawaler, S. D.
Mathur, S.
Jenkins, J. M.
TI Kepler Detected Gravity-Mode Period Spacings in a Red Giant Star
SO SCIENCE
LA English
DT Article
C1 [Beck, P. G.; Carrier, F.; De Ridder, J.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Bedding, T. R.; Stello, D.; White, T. R.; Huber, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Mosser, B.] Univ Paris 07, Univ Paris 06, Lab Etud Spatiales & Instrumentat Astrophys, Observ Paris,CNRS, F-92195 Meudon, France.
[Garcia, R. A.] Univ Paris Diderot, Lab Astrophys Instrumentat & Modelisat, Inst Rech Lois Fondamentales Univers, Serv Astrophys,Direct Sci Mat,CEA,CNRS,Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Kallinger, T.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hekker, S.; Elsworth, Y.; Chaplin, W. J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Hekker, S.; Frandsen, S.] Univ Amsterdam, Astron Inst, NL-1090 GE Amsterdam, Netherlands.
[Kjeldsen, H.; Christensen-Dalsgaard, J.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Aerts, C.] Radboud Univ Nijmegen, Dept Astrophys, Inst Math Astrophys & Particle Phys, NL-6500 GL Nijmegen, Netherlands.
[Dupret, M-A; Montalban, J.; Miglio, A.; Noels, A.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Jenkins, J. M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Beck, PG (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
EM paul.beck@ster.kuleuven.be
OI Kallinger, Thomas/0000-0003-3627-2561; Bedding,
Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Garcia,
Rafael/0000-0002-8854-3776; Kawaler, Steven/0000-0002-6536-6367
FU NASA's Science Mission Directorate; European Community, European
Research Council [227224]
FX We acknowledge the work of the team behind Kepler. Funding for the
Kepler mission is provided by NASA's Science Mission Directorate. We
received funding from the European Community's 7th Framework Programme,
European Research Council grant no. 227224 (PROSPERITY). All authors
thank their national funding agencies.
NR 4
TC 118
Z9 118
U1 2
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 APR 8
PY 2011
VL 332
IS 6026
BP 205
EP 205
DI 10.1126/science.1201939
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 746MM
UT WOS:000289251100041
PM 21415318
ER
PT J
AU Chaplin, WJ
Kjeldsen, H
Christensen-Dalsgaard, J
Basu, S
Miglio, A
Appourchaux, T
Bedding, TR
Elsworth, Y
Garcia, RA
Gilliland, RL
Girardi, L
Houdek, G
Karoff, C
Kawaler, SD
Metcalfe, TS
Molenda-Zakowicz, J
Monteiro, MJPFG
Thompson, MJ
Verner, GA
Ballot, J
Bonanno, A
Brandao, IM
Broomhall, AM
Bruntt, H
Campante, TL
Corsaro, E
Creevey, OL
Dogan, G
Esch, L
Gai, N
Gaulme, P
Hale, SJ
Handberg, R
Hekker, S
Huber, D
Jimenez, A
Mathur, S
Mazumdar, A
Mosser, B
New, R
Pinsonneault, MH
Pricopi, D
Quirion, PO
Regulo, C
Salabert, D
Serenelli, AM
Aguirre, VS
Sousa, SG
Stello, D
Stevens, IR
Suran, MD
Uytterhoeven, K
White, TR
Borucki, WJ
Brown, TM
Jenkins, JM
Kinemuchi, K
Van Cleve, J
Klaus, TC
AF Chaplin, W. J.
Kjeldsen, H.
Christensen-Dalsgaard, J.
Basu, S.
Miglio, A.
Appourchaux, T.
Bedding, T. R.
Elsworth, Y.
Garcia, R. A.
Gilliland, R. L.
Girardi, L.
Houdek, G.
Karoff, C.
Kawaler, S. D.
Metcalfe, T. S.
Molenda-Zakowicz, J.
Monteiro, M. J. P. F. G.
Thompson, M. J.
Verner, G. A.
Ballot, J.
Bonanno, A.
Brandao, I. M.
Broomhall, A-M
Bruntt, H.
Campante, T. L.
Corsaro, E.
Creevey, O. L.
Dogan, G.
Esch, L.
Gai, N.
Gaulme, P.
Hale, S. J.
Handberg, R.
Hekker, S.
Huber, D.
Jimenez, A.
Mathur, S.
Mazumdar, A.
Mosser, B.
New, R.
Pinsonneault, M. H.
Pricopi, D.
Quirion, P-O
Regulo, C.
Salabert, D.
Serenelli, A. M.
Aguirre, V. Silva
Sousa, S. G.
Stello, D.
Stevens, I. R.
Suran, M. D.
Uytterhoeven, K.
White, T. R.
Borucki, W. J.
Brown, T. M.
Jenkins, J. M.
Kinemuchi, K.
Van Cleve, J.
Klaus, T. C.
TI Ensemble Asteroseismology of Solar-Type Stars with the NASA Kepler
Mission
SO SCIENCE
LA English
DT Article
ID SUN-LIKE STAR; RED GIANTS; OSCILLATIONS; COROT; AMPLITUDES; ISOCHRONES;
RADIUS; CYCLE; DEEP
AB In addition to its search for extrasolar planets, the NASA Kepler mission provides exquisite data on stellar oscillations. We report the detections of oscillations in 500 solar-type stars in the Kepler field of view, an ensemble that is large enough to allow statistical studies of intrinsic stellar properties (such as mass, radius, and age) and to test theories of stellar evolution. We find that the distribution of observed masses of these stars shows intriguing differences to predictions from models of synthetic stellar populations in the Galaxy.
C1 [Chaplin, W. J.; Miglio, A.; Elsworth, Y.; Verner, G. A.; Broomhall, A-M; Hale, S. J.; Hekker, S.; Stevens, I. R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Kjeldsen, H.; Christensen-Dalsgaard, J.; Karoff, C.; Bruntt, H.; Campante, T. L.; Dogan, G.; Handberg, R.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Basu, S.; Esch, L.; Gai, N.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Miglio, A.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege 1, Belgium.
[Appourchaux, T.; Gaulme, P.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Bedding, T. R.; Huber, D.; Stello, D.; White, T. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Garcia, R. A.; Uytterhoeven, K.] Univ Paris Diderot, Inst Rech Lois Fondamentales Univers, Lab Astrophys Instrumentat & Modelisat, Direct Sci Mat,CEA,CNRS,Serv Astrophys,Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Girardi, L.] Ist Nazl Astrofis INAF, Osservatorio Astron Padova, I-35122 Padua, Italy.
[Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Metcalfe, T. S.; Thompson, M. J.; Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland.
[Monteiro, M. J. P. F. G.; Brandao, I. M.; Campante, T. L.; Sousa, S. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Monteiro, M. J. P. F. G.; Brandao, I. M.; Campante, T. L.; Sousa, S. G.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
[Verner, G. A.] Univ London, Astron Unit, London E1 4NS, England.
[Ballot, J.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Bonanno, A.; Corsaro, E.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Creevey, O. L.; Jimenez, A.; Regulo, C.; Salabert, D.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Creevey, O. L.; Jimenez, A.; Regulo, C.; Salabert, D.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Gai, N.] Dezhou Univ, Dept Phys, Dezhou 253023, Peoples R China.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Mazumdar, A.] Homi Bhabha Ctr Sci Educ, Bombay 400088, Maharashtra, India.
[Mosser, B.] Univ Paris 07, Univ Paris 06, Lab Etud Spatiales & Instrumentat Astrophys, Observ Paris,CNRS, F-92195 Meudon, France.
[New, R.] Sheffield Hallam Univ, Fac Arts Comp Engn & Sci, Mat Engn Res Inst, Sheffield S1 1WB, S Yorkshire, England.
[Pinsonneault, M. H.] Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA.
[Pricopi, D.; Suran, M. D.] Acad Romana, Astron Inst, RO-40557 Bucharest, Romania.
[Quirion, P-O] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada.
[Serenelli, A. M.] Fac Ciencies, Inst Estudis Espacials Catalunya, Inst Ciencias Espacio, Bellaterra 08193, Spain.
[Aguirre, V. Silva] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Borucki, W. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Jenkins, J. M.; Van Cleve, J.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Kinemuchi, K.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Klaus, T. C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
EM w.j.chaplin@bham.ac.uk
RI Ballot, Jerome/G-1019-2010; PRICOPI, Dumitru/C-4358-2011; Mazumdar,
Anwesh/B-1588-2012; Sousa, Sergio/I-7466-2013; Brandao, Isa/M-5172-2013;
Monteiro, Mario J.P.F.G./B-4715-2008; Basu, Sarbani/B-8015-2014; Hale,
Steven/E-3472-2015
OI Bedding, Timothy/0000-0001-5943-1460; Metcalfe,
Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965;
Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776;
Serenelli, Aldo/0000-0001-6359-2769; Handberg,
Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367;
Mazumdar, Anwesh/0000-0003-2409-2942; Bonanno,
Alfio/0000-0003-3175-9776; Sousa, Sergio/0000-0001-9047-2965; Brandao,
Isa/0000-0002-1153-0942; Monteiro, Mario J.P.F.G./0000-0003-0513-8116;
Basu, Sarbani/0000-0002-6163-3472; Hale, Steven/0000-0002-6402-8382
FU NASA's Science Mission Directorate
FX Kepler is a NASA discovery class mission, which was launched in March
2009 and whose funding is provided by NASA's Science Mission
Directorate. The authors thank the entire Kepler team, without whom
these results would not be possible. The asteroseismology program of
Kepler is being conducted by the Kepler Asteroseismic Science
Consortium.
NR 32
TC 174
Z9 175
U1 2
U2 27
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 APR 8
PY 2011
VL 332
IS 6026
BP 213
EP 216
DI 10.1126/science.1201827
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 746MM
UT WOS:000289251100044
PM 21474754
ER
PT J
AU Derekas, A
Kiss, LL
Borkovits, T
Huber, D
Lehmann, H
Southworth, J
Bedding, TR
Balam, D
Hartmann, M
Hrudkova, M
Ireland, MJ
Kovacs, J
Mezo, G
Moor, A
Niemczura, E
Sarty, GE
Szabo, GM
Szabo, R
Telting, JH
Tkachenko, A
Uytterhoeven, K
Benko, JM
Bryson, ST
Maestro, V
Simon, AE
Stello, D
Schaefer, G
Aerts, C
ten Brummelaar, TA
De Cat, P
McAlister, HA
Maceroni, C
Merand, A
Still, M
Sturmann, J
Sturmann, L
Turner, N
Tuthill, PG
Christensen-Dalsgaard, J
Gilliland, RL
Kjeldsen, H
Quintana, EV
Tenenbaum, P
Twicken, JD
AF Derekas, A.
Kiss, L. L.
Borkovits, T.
Huber, D.
Lehmann, H.
Southworth, J.
Bedding, T. R.
Balam, D.
Hartmann, M.
Hrudkova, M.
Ireland, M. J.
Kovacs, J.
Mezo, Gy.
Moor, A.
Niemczura, E.
Sarty, G. E.
Szabo, Gy. M.
Szabo, R.
Telting, J. H.
Tkachenko, A.
Uytterhoeven, K.
Benko, J. M.
Bryson, S. T.
Maestro, V.
Simon, A. E.
Stello, D.
Schaefer, G.
Aerts, C.
ten Brummelaar, T. A.
De Cat, P.
McAlister, H. A.
Maceroni, C.
Merand, A.
Still, M.
Sturmann, J.
Sturmann, L.
Turner, N.
Tuthill, P. G.
Christensen-Dalsgaard, J.
Gilliland, R. L.
Kjeldsen, H.
Quintana, E. V.
Tenenbaum, P.
Twicken, J. D.
TI HD 181068: A Red Giant in a Triply Eclipsing Compact Hierarchical Triple
System
SO SCIENCE
LA English
DT Article
ID STARS; BINARIES; SCIENCE
AB Hierarchical triple systems comprise a close binary and a more distant component. They are important for testing theories of star formation and of stellar evolution in the presence of nearby companions. We obtained 218 days of Kepler photometry of HD 181068 (magnitude of 7.1), supplemented by ground-based spectroscopy and interferometry, which show it to be a hierarchical triple with two types of mutual eclipses. The primary is a red giant that is in a 45-day orbit with a pair of red dwarfs in a close 0.9-day orbit. The red giant shows evidence for tidally induced oscillations that are driven by the orbital motion of the close pair. HD 181068 is an ideal target for studies of dynamical evolution and testing tidal friction theories in hierarchical triple systems.
C1 [Derekas, A.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary.
[Derekas, A.; Kiss, L. L.; Mezo, Gy.; Moor, A.; Szabo, Gy. M.; Szabo, R.; Benko, J. M.; Simon, A. E.] Hungarian Acad Sci, Konkoly Observ Budapest, H-1525 Budapest, Hungary.
[Kiss, L. L.; Huber, D.; Bedding, T. R.; Ireland, M. J.; Maestro, V.; Stello, D.; Tuthill, P. G.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Borkovits, T.] Baja Astron Observ, H-6500 Baja, Hungary.
[Borkovits, T.] Eotvos Jozsef Coll, H-6500 Baja, Hungary.
[Lehmann, H.; Hartmann, M.; Hrudkova, M.; Tkachenko, A.] Thuringer Landessternwarte TLS Tautenburg, Karl Schwarzschild Observ, D-07778 Tautenburg, Germany.
[Southworth, J.] Univ Keele, Astrophys Grp, Newcastle Under Lyme ST5 5BG, Staffs, England.
[Balam, D.] Dominion Astrophys Observ, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Kovacs, J.] Eotvos Lorand Univ, Gothard Observ, H-9704 Szombathely, Hungary.
[Niemczura, E.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland.
[Sarty, G. E.] Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK S7N 5A5, Canada.
[Telting, J. H.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain.
[Uytterhoeven, K.] Univ Paris Diderot, Lab Astrophys Instrumentat & Modelisat, Inst Rech Lois Fondamentales Univers, Direct Sci Mat,CEA,CNRS,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Uytterhoeven, K.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany.
[Bryson, S. T.; Still, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schaefer, G.; ten Brummelaar, T. A.; McAlister, H. A.; Sturmann, J.; Sturmann, L.; Turner, N.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
[Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Aerts, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[De Cat, P.] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Maceroni, C.] Osserv Astron Roma, Ist Nazl Astrofis INAF, I-00040 Monteporzio C, Italy.
[Merand, A.] European So Observ, Santiago 19, Chile.
[Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Quintana, E. V.; Tenenbaum, P.; Twicken, J. D.] SETI Inst, Moffett Field, CA 94035 USA.
RP Derekas, A (reprint author), Eotvos Lorand Univ, Dept Astron, Budapest, Hungary.
EM derekas@konkoly.hu
RI Szabo, Gyula/A-8310-2012; Derekas, Aliz/G-2091-2016;
OI Derekas, Aliz/0000-0002-6526-9444; Sarty, Gordon/0000-0001-5516-7869;
Benko, Jozsef/0000-0003-3851-6603; Bedding, Timothy/0000-0001-5943-1460;
Szabo, Robert/0000-0002-3258-1909; Bedding, Tim/0000-0001-5222-4661
FU NASA's Science Mission Directorate; Hungarian Scientific Research Fund
(OTKA) [K76816, K83790, MB08C 81013]; Hungarian Academy of Sciences;
Magyary Zoltan Higher Educational Public Foundation; American
Astronomical Society; NSF [AST09-08253]; W. M. Keck Foundation; NASA
Exoplanet Science Center; Deutsche Forschungsgemeinschaft [HA 3279/5-1];
European Research Council (ERC) under the European Community [227224]
FX A.D. is a Magyary Zoltan Postdoctoral Research Fellow. Funding for this
Discovery mission is provided by NASA's Science Mission Directorate. The
authors gratefully acknowledge the entire Kepler team, whose outstanding
efforts have made these results possible. This project has been
supported by Hungarian Scientific Research Fund (OTKA) grants K76816,
K83790, and MB08C 81013; the "Lendulet" Program of the Hungarian Academy
of Sciences; and the Magyary Zoltan Higher Educational Public
Foundation. The DAO observations were supported by an American
Astronomical Society Small Research Grant. The CHARA Array is owned by
Georgia State University. Additional funding for the CHARA Array is
provided by NSF under grant AST09-08253, the W. M. Keck Foundation, and
the NASA Exoplanet Science Center. TLS observations were done as a part
of the Deutsche Forschungsgemeinschaft grant HA 3279/5-1. For her
research, C. A. received funding from the European Research Council
(ERC) under the European Community's Seventh Framework Programme
(FP7/2007-2013)/ERC grant agreement no. 227224 (Prosperity).
NR 19
TC 51
Z9 51
U1 1
U2 4
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD APR 8
PY 2011
VL 332
IS 6026
BP 216
EP 218
DI 10.1126/science.1201762
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 746MM
UT WOS:000289251100045
PM 21474755
ER
PT J
AU Lin, RQ
Kuang, WJ
AF Lin, Ray-Qing
Kuang, Weijia
TI A fully nonlinear, dynamically consistent numerical model for solid-body
ship motion. I. Ship motion with fixed heading
SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING
SCIENCES
LA English
DT Article
DE ship motion; nonlinearity; hydrodynamics; solid body; numerical model
ID WAVES
AB In this paper, we describe the details of our numerical model for simulating ship solid-body motion in a given environment. In this model, the fully nonlinear dynamical equations governing the time-varying solid-body ship motion under the forces arising from ship-wave interactions are solved with given initial conditions. The net force and moment (torque) on the ship body are directly calculated via integration of the hydrodynamic pressure over the wetted surface and the buoyancy effect from the underwater volume of the actual ship hull with a hybrid finite-difference/finite-element method. Neither empirical nor free parametrization is introduced in this model, i.e. no a priori experimental data are needed for modelling. This model is benchmarked with many experiments of various ship hulls for heave, roll and pitch motion. In addition to the benchmark cases, numerical experiments are also carried out for strongly nonlinear ship motion with a fixed heading. These new cases demonstrate clearly the importance of nonlinearities in ship motion modelling.
C1 [Lin, Ray-Qing] NSWCCD, Carderock Div, Bethesda, MD USA.
[Kuang, Weijia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lin, RQ (reprint author), NSWCCD, Carderock Div, Bethesda, MD USA.
EM ray.lin@navy.mil
RI Kuang, Weijia/K-5141-2012
OI Kuang, Weijia/0000-0001-7786-6425
FU David Taylor Model Basin, Carderock Division; NASA ESIP; MFRP
FX R.L. is supported by ILIR programme from the David Taylor Model Basin,
Carderock Division. W. K. is supported by NASA ESIP and MFRP. We thank
T. Applebee and J. Gorski of the David Taylor Model Basin,
Hydromechanics Department for their help on this work.
NR 26
TC 5
Z9 5
U1 0
U2 1
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-5021
J9 P ROY SOC A-MATH PHY
JI Proc. R. Soc. A-Math. Phys. Eng. Sci.
PD APR 8
PY 2011
VL 467
IS 2128
BP 911
EP 927
DI 10.1098/rspa.2010.0310
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 726OX
UT WOS:000287735600001
ER
PT J
AU Qu, TD
Gao, S
Fukumori, I
AF Qu, Tangdong
Gao, Shan
Fukumori, Ichiro
TI What governs the North Atlantic salinity maximum in a global GCM?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SEA-SURFACE SALINITY; TROPICAL ATLANTIC; MIXED-LAYER; OCEAN; MODEL;
TRENDS; CLIMATOLOGY; VARIABILITY
AB Taking advantage of the rapid advance in ocean modeling, this study investigates the sea surface salinity maximum in the North Atlantic, using results from a model of the Consortium for Estimating the Circulation and Climate of the Ocean (ECCO). Salinity budget terms were computed at the model's integration time step and archived as monthly averages. The simulated mixed layer salinity budget provides the first quantitative evidence for the ocean's role in governing the sea surface salinity maximum in the North Atlantic. Our analysis reveals that ocean dynamics explains about half of the sea surface salinity variance, being of equal importance as surface forcing. The sea surface salinity maximum varies both seasonally and interannually, as a consequence of interplay among surface flux, advection, and vertical entrainment. Contribution from eddies and small-scale processes is relatively weak but not negligible. These results may provide useful hints for the design and interpretation of future observations in the region. Citation: Qu, T., S. Gao, and I. Fukumori (2011), What governs the North Atlantic salinity maximum in a global GCM?, Geophys. Res. Lett., 38, L07602, doi:10.1029/2011GL046757.
C1 [Qu, Tangdong] Univ Hawaii Manoa, SOEST, Int Pacific Res Ctr, Honolulu, HI 96822 USA.
[Gao, Shan] Chinese Acad Sci, Inst Oceanol, Qingdao 266071, Shandong, Peoples R China.
[Fukumori, Ichiro] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Qu, TD (reprint author), Univ Hawaii Manoa, SOEST, Int Pacific Res Ctr, 1680 East West Rd, Honolulu, HI 96822 USA.
EM tangdong@hawaii.edu
RI Gao, Shan/H-7959-2013
OI Gao, Shan/0000-0003-4510-5028
FU NASA; JAMSTEC; NOAA; National Science Foundation of China [40876011]
FX This research was supported by NASA as part of the Aquarius Science Team
investigation. Additional support for T. Qu was provided by JAMSTEC,
NASA, and NOAA through their sponsorship of research activities at the
IPRC. S. Gao was supported by the National Science Foundation of China
through grant 40876011. The authors are grateful to F. Bingham, L. Yu,
A. Gordon, P. Hacker, and E. Lindstrom for valuable discussions and to
two anonymous reviewers for thoughtful comments on the manuscript. SOEST
contribution 8104 and IPRC contribution IPRC-763.
NR 28
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U1 1
U2 8
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 APR 7
PY 2011
VL 38
AR L07602
DI 10.1029/2011GL046757
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 747YK
UT WOS:000289357000001
ER
PT J
AU Martini, M
Allen, DJ
Pickering, KE
Stenchikov, GL
Richter, A
Hyer, EJ
Loughner, CP
AF Martini, Matus
Allen, Dale J.
Pickering, Kenneth E.
Stenchikov, Georgiy L.
Richter, Andreas
Hyer, Edward J.
Loughner, Christopher P.
TI The impact of North American anthropogenic emissions and lightning on
long-range transport of trace gases and their export from the continent
during summers 2002 and 2004
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPOSPHERIC OZONE PRODUCTION; OPTICAL TRANSIENT DETECTOR; REGIONAL
AIR-POLLUTION; EASTERN UNITED-STATES; VERTICAL-DISTRIBUTION; GENERATED
NOX; SURFACE OZONE; SCALE-MODEL; STERAO-A; CHEMISTRY
AB We analyze the contribution of North American (NA) lightning and anthropogenic emissions to ozone concentrations, radiative forcing, and export fluxes from North America during summers 2002 and 2004 using the University of Maryland Chemical Transport Model (UMD-CTM) driven by GEOS-4 reanalysis. Reduced power plant emissions (NOx SIP Call) and cooler temperatures in 2004 compared to 2002 resulted in lower ambient ozone concentrations over the eastern United States. Lightning flash rates in early summer 2004 were 50% higher than 2002 over the United States. Over the North Atlantic, changes in ozone column between early summer 2002 and 2004 due to changes in lightning and meteorology exceeded the change due to emission reductions by a factor of 7. Late summer changes in lightning had a much smaller impact on ozone columns. In summer 2004, net downward radiative flux at the tropopause due to ozone produced from anthropogenic emissions ranged from 0.15 to 0.30 W m(-2) across the North Atlantic, while that due to ozone produced from lightning NO emissions ranged from 0.20 to 0.50 W m(-2). Enhanced lofting of polluted air followed by stronger westerly winds led to more net export of NOx, NOy, and ozone in early summer 2004 than 2002 despite reduced anthropogenic emissions. Ozone export fluxes across the eastern NA boundary due to anthropogenic emissions were factors of 1.6 and 2 larger than those due to lightning in 2004 and 2002, respectively. Doubling the NA lightning NO source increased downwind ozone enhancements due to lightning NO emissions by one third.
C1 [Martini, Matus; Allen, Dale J.; Loughner, Christopher P.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Hyer, Edward J.] USN, UCAR Visiting Scientist Program, Res Lab, Monterey, CA 93943 USA.
[Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Richter, Andreas] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany.
[Stenchikov, Georgiy L.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA.
[Stenchikov, Georgiy L.] King Abdullah Univ Sci & Technol, Thuwal, Saudi Arabia.
RP Martini, M (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM martini@atmos.umd.edu
RI Hyer, Edward/E-7734-2011; Pickering, Kenneth/E-6274-2012; Georgiy,
Stenchikov/J-8569-2013; Richter, Andreas/C-4971-2008; Allen,
Dale/F-7168-2010;
OI Hyer, Edward/0000-0001-8636-2026; Loughner,
Christopher/0000-0002-3833-2014; Richter, Andreas/0000-0003-3339-212X;
Allen, Dale/0000-0003-3305-9669; Stenchikov, Georgiy
Lvovich/0000-0001-9033-4925; Martini, Matus/0000-0003-0459-4988
FU NASA [NNG04GD32G, NNG06GE01G, NNG06GB52G]
FX This work was funded under NASA grants NNG04GD32G and NNG06GE01G
(Interdisciplinary Science Investigation) and under NASA grant
NNG06GB52G from the Tropospheric Chemistry Program. Model simulations
have been conducted at NCCS at NASA Goddard Space Flight Center. We
thank the INTEX-A science team for the aircraft measurements and Anne
Thompson for IONS measurements. The NLDN data were collected by Vaisala,
Inc., and archived by NASA Marshall Space Flight Center. OTD/LIS data
were processed by NASA Marshall. We thank Owen Cooper for the IC/CG
ratios prepared by Dennis Boccippio. We thank Arlene Fiore and two
anonymous reviewers for their helpful comments. We also thank Ross
Salawitch and Amanda Evans for their revisions and comments.
NR 90
TC 6
Z9 6
U1 1
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 7
PY 2011
VL 116
AR D07305
DI 10.1029/2010JD014305
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 747ZN
UT WOS:000289359900001
ER
PT J
AU Abbasi, R
Abdou, Y
Abu-Zayyad, T
Adams, J
Aguilar, JA
Ahlers, M
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Bay, R
Alba, JLB
Beattie, K
Beatty, JJ
Bechet, S
Becker, JK
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Braun, J
Brown, AM
Buitink, S
Carson, M
Chirkin, D
Christy, B
Clem, J
Clevermann, F
Cohen, S
Colnard, C
Cowen, DF
D'Agostino, MV
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
Demirors, L
Depaepe, O
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dierckxsens, M
Dreyer, J
Dumm, JP
Ehrlich, R
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feusels, T
Filimonov, K
Finley, C
Fischer-Wasels, T
Foerster, MM
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Geisler, M
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Grant, D
Griesel, T
Gross, A
Grullon, S
Gurtner, M
Ha, C
Hallgren, A
Halzen, F
Han, K
Hanson, K
Heinen, D
Helbing, K
Herquet, P
Hickford, S
Hill, GC
Hoffman, KD
Homeier, A
Hoshina, K
Hubert, D
Huelsnitz, W
Hulss, JP
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kemming, N
Kenny, P
Kiryluk, J
Kislat, F
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, S
Koskinen, DJ
Kowalski, M
Kowarik, T
Krasberg, M
Krings, T
Kroll, G
Kuehn, K
Kuwabara, T
Labare, M
Lafebre, S
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lehmann, R
Lunemann, J
Madsen, J
Majumdar, P
Marotta, A
Maruyama, R
Mase, K
Matis, HS
Meagher, K
Merck, M
Meszaros, P
Meures, T
Middell, E
Milke, N
Miller, J
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Nam, JW
Naumann, U
Niessen, P
Nygren, DR
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Ono, M
Panknin, S
Paul, L
de los Heros, CP
Petrovic, J
Piegsa, A
Pieloth, D
Porrata, R
Posselt, J
Price, PB
Prikockis, M
Przybylski, GT
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Rodrigues, JP
Roth, P
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Schmidt, T
Schoenwald, A
Schukraft, A
Schultes, A
Schulz, O
Schunck, M
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Slipak, A
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stephens, G
Stezelberger, T
Stokstad, RG
Stoyanov, S
Strahler, EA
Straszheim, T
Sullivan, GW
Swillens, Q
Taavola, H
Taboada, I
Tamburro, A
Tarasova, O
Tepe, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Tosi, D
Turcan, D
van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Voigt, B
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wischnewski, R
Wissing, H
Wolf, M
Woschnagg, K
Xu, C
Xu, XW
Yodh, G
Yoshida, S
Zarzhitsky, P
AF Abbasi, R.
Abdou, Y.
Abu-Zayyad, T.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Bay, R.
Alba, J. L. Bazo
Beattie, K.
Beatty, J. J.
Bechet, S.
Becker, J. K.
Becker, K. -H.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brown, A. M.
Buitink, S.
Carson, M.
Chirkin, D.
Christy, B.
Clem, J.
Clevermann, F.
Cohen, S.
Colnard, C.
Cowen, D. F.
D'Agostino, M. V.
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
Demiroers, L.
Depaepe, O.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dierckxsens, M.
Dreyer, J.
Dumm, J. P.
Ehrlich, R.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feusels, T.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Geisler, M.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Grant, D.
Griesel, T.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Heinen, D.
Helbing, K.
Herquet, P.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Homeier, A.
Hoshina, K.
Hubert, D.
Huelsnitz, W.
Huelss, J. -P.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Joseph, J. M.
Kampert, K. -H.
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
Kemming, N.
Kenny, P.
Kiryluk, J.
Kislat, F.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Krings, T.
Kroll, G.
Kuehn, K.
Kuwabara, T.
Labare, M.
Lafebre, S.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Lehmann, R.
Luenemann, J.
Madsen, J.
Majumdar, P.
Marotta, A.
Maruyama, R.
Mase, K.
Matis, H. S.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Middell, E.
Milke, N.
Miller, J.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Nam, J. W.
Naumann, U.
Niessen, P.
Nygren, D. R.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Ono, M.
Panknin, S.
Paul, L.
de los Heros, C. Perez
Petrovic, J.
Piegsa, A.
Pieloth, D.
Porrata, R.
Posselt, J.
Price, P. B.
Prikockis, M.
Przybylski, G. T.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Rodrigues, J. P.
Roth, P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Schmidt, T.
Schoenwald, A.
Schukraft, A.
Schultes, A.
Schulz, O.
Schunck, M.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Slipak, A.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stephens, G.
Stezelberger, T.
Stokstad, R. G.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Sullivan, G. W.
Swillens, Q.
Taavola, H.
Taboada, I.
Tamburro, A.
Tarasova, O.
Tepe, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Tosi, D.
Turcan, D.
van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Voigt, B.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Weaver, C.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Wolf, M.
Woschnagg, K.
Xu, C.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
TI Limits on Neutrino Emission from Gamma-Ray Bursts with the 40 String
IceCube Detector
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID HIGH-ENERGY NEUTRINOS; MUON NEUTRINOS; SEARCH; AMANDA
AB IceCube has become the first neutrino telescope with a sensitivity below the TeV neutrino flux predicted from gamma-ray bursts if gamma-ray bursts are responsible for the observed cosmic-ray flux above 10(18) eV. Two separate analyses using the half-complete IceCube detector, one a dedicated search for neutrinos from p gamma interactions in the prompt phase of the gamma-ray burst fireball and the other a generic search for any neutrino emission from these sources over a wide range of energies and emission times, produced no evidence for neutrino emission, excluding prevailing models at 90% confidence.
C1 [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Heinen, D.; Huelss, J. -P.; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Kappes, A.; Kemming, N.; Kolanoski, H.; Lehmann, R.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium.
[Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium.
[Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Braun, J.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kelley, J. L.; Krasberg, M.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, C.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Tarasova, O.; Tosi, D.; Voigt, B.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
[Montaruli, T.] Univ Bari, I-70126 Bari, Italy.
[Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Meagher, K (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
RI Tamburro, Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren,
Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014;
Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015;
Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty,
James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Kowalski,
Marek/G-5546-2012; Taavola, Henric/B-4497-2011;
OI Auffenberg, Jan/0000-0002-1185-9094; Koskinen,
David/0000-0002-0514-5917; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
Actis, Oxana/0000-0001-8851-3983; Wiebusch,
Christopher/0000-0002-6418-3008; Ter-Antonyan,
Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479; Perez
de los Heros, Carlos/0000-0002-2084-5866; Taavola,
Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Carson,
Michael/0000-0003-0400-7819; Hubert, Daan/0000-0002-4365-865X;
Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886
FU U.S. NSF-Office of Polar Programs; U.S. NSF-Physics Division; University
of Wisconsin Alumni Research Foundation; GLOW and OSG grids; U.S. DOE;
NERSCC; LONI grid; NSERC, Canada; Swedish Research Council; Swedish
Polar Research Secretariat; SNIC; K. and A. Wallenberg Foundation,
Sweden; German Ministry for Education and Research; Deutsche
Forschungsgemeinschaft; FSR; FWO Odysseus; IWT; BELSPO, Belgium; Marsden
Fund, New Zealand; JSPS, Japan; SNSF, Switzerland; EU; Capes Foundation,
Brazil; NSF GRFP
FX We acknowledge support from the following agencies: U.S. NSF-Office of
Polar Programs, U.S. NSF-Physics Division, University of Wisconsin
Alumni Research Foundation, the GLOW and OSG grids; U.S. DOE, NERSCC,
the LONI grid; NSERC, Canada; Swedish Research Council, Swedish Polar
Research Secretariat, SNIC, K. and A. Wallenberg Foundation, Sweden;
German Ministry for Education and Research, Deutsche
Forschungsgemeinschaft; FSR, FWO Odysseus, IWT, BELSPO, Belgium; Marsden
Fund, New Zealand; JSPS, Japan; SNSF, Switzerland. A. Gross is supported
by the EU Marie Curie OIF Program, J. P. R. by the Capes Foundation,
Brazil, and N. W. by the NSF GRFP.
NR 18
TC 74
Z9 76
U1 1
U2 9
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 7
PY 2011
VL 106
IS 14
AR 141101
DI 10.1103/PhysRevLett.106.141101
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 747XY
UT WOS:000289355800002
PM 21561178
ER
PT J
AU Falconer, D
Barghouty, AF
Khazanov, I
Moore, R
AF Falconer, David
Barghouty, Abdulnasser F.
Khazanov, Igor
Moore, Ron
TI A tool for empirical forecasting of major flares, coronal mass
ejections, and solar particle events from a proxy of active-region free
magnetic energy
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID VECTOR MAGNETOGRAMS; FIELD; NONPOTENTIALITY; PRODUCTIVITY; HELIOSPHERE;
PREDICTION; TIME
AB This paper describes a new forecasting tool developed for and currently being tested by NASA's Space Radiation Analysis Group (SRAG) at Johnson Space Center, which is responsible for the monitoring and forecasting of radiation exposure levels of astronauts. The new software tool is designed for the empirical forecasting of M- and X-class flares, coronal mass ejections, and solar energetic particle events. For each type of event, the algorithm is based on the empirical relationship between the event rate and a proxy of the active region's free magnetic energy. Each empirical relationship is determined from a data set of similar to 40,000 active-region magnetograms from similar to 1300 active regions observed by SOHO/Michelson Doppler Imager (MDI) that have known histories of flare, coronal mass ejection, and solar energetic particle event production. The new tool automatically extracts each strong-field magnetic area from an MDI full-disk magnetogram, identifies each as a NOAA active region, and measures the proxy of the active region's free magnetic energy from the extracted magnetogram. For each active region, the empirical relationship is then used to convert the free-magnetic-energy proxy into an expected event rate. The expected event rate in turn can be readily converted into the probability that the active region will produce such an event in a given forward time window. Descriptions of the data sets, algorithm, and software in addition to sample applications and a validation test are presented. Further development and transition of the new tool in anticipation of SDO/HMI are briefly discussed.
C1 [Falconer, David; Barghouty, Abdulnasser F.; Moore, Ron] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Falconer, David; Khazanov, Igor] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Falconer, David] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
RP Falconer, D (reprint author), NASA, Space Sci Off, George C Marshall Space Flight Ctr, Mail Code VP62, Huntsville, AL 35812 USA.
EM david.a.falconer@nasa.gov
FU NASA's Office of Chief Engineer Technical Excellence Initiative; NASA
Heliophysics Division; NSF's Division of Atmospheric Sciences; AFOSR
FX The development of this tool was supported by funding from NASA's Office
of Chief Engineer Technical Excellence Initiative. The science that went
into development of this tool was supported by funding from the NASA
Heliophysics Division, from NSF's Division of Atmospheric Sciences, and
from AFOSR'S MURI Program. We wish to acknowledge the use of both Chris
Balch flare/CME data sets and the CME catalog generated and maintained
at the CDAW Data Center by NASA and The Catholic University of America
in cooperation with the Naval Research Laboratory. The paper has also
been improved by comments of the two anonymous referees.
NR 25
TC 26
Z9 26
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR 7
PY 2011
VL 9
AR S04003
DI 10.1029/2009SW000537
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 747ZV
UT WOS:000289360700001
ER
PT J
AU Wei, CY
Pohorile, A
AF Wei, Chenyu
Pohorile, Andrew
TI Permeation of Nucleosides through Lipid Bilayers
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID FREE-ENERGY CALCULATIONS; RNA WORLD; SIMULATION; LIPOSOMES; MEMBRANE;
SPECTROSCOPY; COMPONENTS; DYNAMICS; VESICLES; MODELS
AB Elucidating mechanisms that facilitate primordial synthesis of information polymers is central to understanding the origins of life. One such mechanism might have been the recently discovered diastereoselectivity of membranes favoring uptake of ribose (Sacerdote, M. G.; Szostak, J. W. Proc. Natl. Acad. Sci. U.S.A. 2005, 102, 6004), which might have promoted its preferential incorporation into nucleic acids. To determine whether the same mechanism was available if nucleosides rather than sugars were supplied to ancestral cells, we carry out molecular dynamics simulations of their permeation through a lipid bilayer. We find that the free energy barriers to permeation of ribo-adenosine and arabino-adenosine through the 1-palmitoyl-2-oleoyl-sn-glycero-3-phosphatidylcholine membrane are quite similar, equal to 10.0 and 10.4 kcal/mol, respectively. The corresponding permeability coefficients are also similar, equal to 9.1 x 10(-7) and 5.3 x 10(-7) cm/s. The 10-fold increase in permeability of membranes to ribose over its diastereomers is not preserved for nucleosides because in contrast to free aldopentoses they exist in the furanose rather than pyranose form. This change eliminates the possibility of forming a network of favorable, intramolecular interactions between exocyclic, hydroxyl groups that stabilizes ribose, but not its diastereomers, inside membranes. Thus, uptake of nutrients provided selective advantage to primordial RNA only if the species absorbed through cell walls were sugars rather than nucleosides.
C1 [Wei, Chenyu; Pohorile, Andrew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wei, Chenyu; Pohorile, Andrew] Univ Calif San Francisco, Dept Pharmaceut Chem, San Francisco, CA 94143 USA.
RP Wei, CY (reprint author), NASA, Ames Res Ctr, Mail Stop 229-1, Moffett Field, CA 94035 USA.
EM Chenyu.Wei@nasa.gov; Andrew.Pohor-ille@nasa.gov
FU NASA Exobiology Program
FX This work was supported by the NASA Exobiology Program. NASA Advanced
Supercomputing (NAS) Division provided computational resources needed to
carry out this study.
NR 53
TC 19
Z9 19
U1 1
U2 67
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1520-6106
J9 J PHYS CHEM B
JI J. Phys. Chem. B
PD APR 7
PY 2011
VL 115
IS 13
BP 3681
EP 3688
DI 10.1021/jp112104r
PG 8
WC Chemistry, Physical
SC Chemistry
GA 741SU
UT WOS:000288885700044
PM 21405137
ER
PT J
AU Choi, YJ
Lu, J
Sohn, HY
Fang, ZZ
Kim, C
Bowman, RC
Hwang, SJ
AF Choi, Young Joon
Lu, Jun
Sohn, Hong Yong
Fang, Zhigang Zak
Kim, Chul
Bowman, Robert C., Jr.
Hwang, Son-Jong
TI Reaction Mechanisms in the Li3AlH6/LiBH4 and Al/LiBH4 Systems for
Reversible Hydrogen Storage. Part 2: Solid-State NMR Studies
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID MAS NMR; LIBH4; AL-27; ALUMINUM; HYDRIDE; AL; BOROHYDRIDES; POWDER; MG;
TI
AB In Part 1, the promising hydrogen storage properties of the combined systems of Li3AlH6/LiBH4 and Al/LiBH4, exhibiting the favorable formation of AlB2 during dehydrogenation, were presented based on TGA and XRD analyses. The present Part 2 describes the characterization of the intermediate and final products of the dehydrogenation and rehydrogenation of the above systems by multinuclear solid-state NMR characterization. This work has also verified that the presence of Al resulted in the re-formation of LiBH4 occurring at a much lower temperature and H-2 pressure, under which conditions the dehydrogenation product from LiBH4 alone does not show any degree of rehydrogenation. NMR studies mainly identified various reaction intermediates for LiBH4 dehydrogenation/rehydrotrnation reactions. Unlike the XRD studies, the AlB2 formation, in particular, could not be unambiguously confirmed by NMR. Al-27 NMR showed that aluminum was mainly involved in various Li-Al alloy formations. The catalytic role of Al in the LiBH4 hydrogen storage reactivity could be achieved by a reversible cycle of the Al + LiH <-> LiAl + 1/2H(2) reaction.
C1 [Choi, Young Joon; Lu, Jun; Sohn, Hong Yong; Fang, Zhigang Zak] Univ Utah, Dept Met Engn, Salt Lake City, UT 84112 USA.
[Kim, Chul; Hwang, Son-Jong] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Bowman, Robert C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sohn, HY (reprint author), Univ Utah, Dept Met Engn, 135 S 1460 E Room, Salt Lake City, UT 84112 USA.
EM h.y.sohn@utah.edu; sonjong@cheme.caltech.edu
FU U.S. Department of Energy (DOE), Office of Energy Efficiency and
Renewable Energy [DE-FC36-05GO15069, DE-Al-01-05EE11105]; National
Science Foundation (NSF) [9724240, DMR-520565]
FX This research was supported by the U.S. Department of Energy (DOE),
Office of Energy Efficiency and Renewable Energy, through the Hydrogen,
Fuel Cells & Infrastructure Technologies Program under Contract Numbers
DE-FC36-05GO15069 (U. Utah) and DE-AI-01-05EE11105 (Jet Propulsion Lab).
The NMR facility at Caltech was supported by the National Science
Foundation (NSF) under Grant Number 9724240 and partially supported by
the MRSEC Program of the NSF under Award Number DMR-520565.
NR 25
TC 24
Z9 24
U1 1
U2 29
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD APR 7
PY 2011
VL 115
IS 13
BP 6048
EP 6056
DI 10.1021/jp109113f
PG 9
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 741SW
UT WOS:000288885900105
ER
PT J
AU Bushnell, D
Garneau, M
Logsdon, JM
Sagdeev, R
Lu, E
Mountain, M
Stephenson, N
AF Bushnell, Dennis
Garneau, Marc
Logsdon, John M.
Sagdeev, Roald
Lu, Ed
Mountain, Matt
Stephenson, Neal
TI NASA: what now?
SO NATURE
LA English
DT Editorial Material
C1 [Bushnell, Dennis] NASA, Langley Res Ctr, Washington, DC 20546 USA.
[Logsdon, John M.] George Washington Univ, Washington, DC 20052 USA.
[Sagdeev, Roald] Russian Space Res Inst, Moscow, Russia.
[Mountain, Matt] NASA, Space Telescope Sci Inst, Washington, DC USA.
RP Bushnell, D (reprint author), NASA, Langley Res Ctr, Washington, DC 20546 USA.
NR 0
TC 1
Z9 1
U1 0
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 7
PY 2011
VL 472
IS 7341
BP 27
EP 29
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 745VV
UT WOS:000289199400016
PM 21475173
ER
PT J
AU Buratti, BJ
Hicks, MD
Nettles, J
Staid, M
Pieters, CM
Sunshine, J
Boardman, J
Stone, TC
AF Buratti, B. J.
Hicks, M. D.
Nettles, J.
Staid, M.
Pieters, C. M.
Sunshine, J.
Boardman, J.
Stone, T. C.
TI A wavelength-dependent visible and infrared spectrophotometric function
for the Moon based on ROLO data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; SATELLITES; PHOTOMETRY;
CLEMENTINE
AB The USGS's Robotic Lunar Observatory (ROLO) dedicated ground-based lunar calibration project obtained photometric observations of the Moon over the spectral range attainable from Earth (0.347-2.39 mu m) and over solar phase angles of 1.55 degrees-97 degrees. From these observations, we derived empirical lunar surface solar phase functions for both the highlands and maria that can be used for a wide range of applications. The functions can be used to correct for the effects of viewing geometry to produce lunar mosaics, spectra, and quick-look products for future lunar missions and ground-based observations. Our methodology can be used for a wide range of objects for which multiply scattered radiation is not significant, including all but the very brightest asteroids and moons.
C1 [Buratti, B. J.; Hicks, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nettles, J.; Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Staid, M.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Boardman, J.] Analyt Imaging & Geophys, Boulder, CO 80303 USA.
[Stone, T. C.] USGS, Flagstaff, AZ 86001 USA.
RP Buratti, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-401, Pasadena, CA 91109 USA.
EM bonnie.j.buratti@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract to the National
Aeronautics and Space Administration. We thank Deborah Domingue for a
detailed review.
NR 24
TC 10
Z9 10
U1 2
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR 5
PY 2011
VL 116
AR E00G03
DI 10.1029/2010JE003724
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 748AA
UT WOS:000289361200001
ER
PT J
AU Parker, ET
Cleaves, HJ
Dworkin, JP
Glavin, DP
Callahan, M
Aubrey, A
Lazcano, A
Bada, JL
AF Parker, Eric T.
Cleaves, Henderson J.
Dworkin, Jason P.
Glavin, Daniel P.
Callahan, Michael
Aubrey, Andrew
Lazcano, Antonio
Bada, Jeffrey L.
TI Primordial synthesis of amines and amino acids in a 1958 Miller H2S-rich
spark discharge experiment
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE prebiotic chemistry; volcano plume chemistry; carbonaceous chondrites
ID EARLY EARTH ATMOSPHERE; LIQUID-CHROMATOGRAPHY; NITROGEN-FIXATION;
PRIMITIVE EARTH; LIFE; CHEMISTRY; ERUPTIONS; SULFUR; ORIGIN; OCEAN
AB Archived samples from a previously unreported 1958 Stanley Miller electric discharge experiment containing hydrogen sulfide (H2S) were recently discovered and analyzed using high-performance liquid chromatography and time-of-flight mass spectrometry. We report here the detection and quantification of primary amine-containing compounds in the original sample residues, which were produced via spark discharge using a gaseous mixture of H2S, CH4, NH3, and CO2. A total of 23 amino acids and 4 amines, including 7 organosulfur compounds, were detected in these samples. The major amino acids with chiral centers are racemic within the accuracy of the measurements, indicating that they are not contaminants introduced during sample storage. This experiment marks the first synthesis of sulfur amino acids from spark discharge experiments designed to imitate primordial environments. The relative yield of some amino acids, in particular the isomers of aminobutyric acid, are the highest ever found in a spark discharge experiment. The simulated primordial conditions used by Miller may serve as a model for early volcanic plume chemistry and provide insight to the possible roles such plumes may have played in abiotic organic synthesis. Additionally, the overall abundances of the synthesized amino acids in the presence of H2S are very similar to the abundances found in some carbonaceous meteorites, suggesting that H2S may have played an important role in prebiotic reactions in early solar system environments.
C1 [Parker, Eric T.; Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA.
[Cleaves, Henderson J.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Dworkin, Jason P.; Glavin, Daniel P.; Callahan, Michael] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Aubrey, Andrew] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[Lazcano, Antonio] Univ Nacl Autonoma Mexico, Fac Ciencias, Mexico City 04510, DF, Mexico.
RP Bada, JL (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, 8615 Kennel Way, La Jolla, CA 92093 USA.
EM jbada@ucsd.edu
RI Callahan, Michael/D-3630-2012; Glavin, Daniel/D-6194-2012; Dworkin,
Jason/C-9417-2012;
OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997;
Cleaves, Henderson/0000-0003-4101-0654
FU National Aeronautics and Space Administration Astrobiology Institute;
Goddard Center for Astrobiology; National Aeronautics and Space
Administration; National Science Foundation [CHE-1004570]
FX Stanley L. Miller passed away on May 20, 2007. Because his research
ushered in the era of experimental studies on the origin of life, we
dedicate this work to his memory. We thank Jamie Elsila for GC-MS
analyses of these residues and Facundo Fernandez and the reviewers for
helpful comments. We deeply appreciate the Mandeville Special
Collections in the University of California, San Diego Geisel Library
for assistance with archiving and retrieving Miller's original
laboratory notebooks. We are grateful for funding support from the
National Aeronautics and Space Administration Astrobiology Institute and
the Goddard Center for Astrobiology. M. C. and H.J.C. acknowledge
support from the National Aeronautics and Space Administration
Postdoctoral Program administered by Oak Ridge Associated Universities.
Assistance with data analysis and figure preparation (A. A.) was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. J.L.B. and H.J.C. are also affiliated with the Center
for Chemical Evolution at the Georgia Institute of Technology, which is
jointly supported by the National Science Foundation and the National
Aeronautics and Space Administration Astrobiology Program, under the
National Science Foundation Grant CHE-1004570.
NR 39
TC 64
Z9 69
U1 10
U2 70
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 APR 5
PY 2011
VL 108
IS 14
BP 5526
EP 5531
DI 10.1073/pnas.1019191108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 746RT
UT WOS:000289265300013
PM 21422282
ER
PT J
AU Kobrick, RL
Klaus, DM
Street, KW
AF Kobrick, Ryan L.
Klaus, David M.
Street, Kenneth W.
TI Standardization of a volumetric displacement measurement for two-body
abrasion scratch test data analysis
SO WEAR
LA English
DT Article
DE Two-body abrasion; Scratch testing; Lunar dust; Surface topography;
Profilometry; Surface analysis
ID PARALLEL GROOVES; GENERATION; SURFACES
AB A limitation has been identified in the existing test standards used for making controlled, two-body abrasion scratch measurements (ASTM Standard G 171) based solely on the width of the resultant score on the surface of the material. A new, more robust method is proposed to complement the current two-body scratch test standard for analyzing a surface scratch that takes into account the full three-dimensional (3D) profile of the displaced material. To accomplish this, a set of four volume displacement metrics are systematically defined by normalizing the overall surface profile to statistically denote the area of relevance, termed the 'Zone of Interaction' (ZOI). From this baseline, depth of the trough and height of the ploughed material are factored into the overall deformation assessment. A complete set of roughness parameters are calculated on the fresh surface and resulting abraded surface to aid in shape change characterization of the material. Proof of concept data were collected and analyzed to demonstrate the performance of this proposed methodology. This technique takes advantage of advanced imaging capabilities that now allow resolution of the scratched surface to be quantified in greater detail than was previously achievable. A quantified understanding of fundamental particle-material interaction is critical to anticipating how well components can withstand prolonged use in highly abrasive environments, specifically for our intended applications on the surface of the moon and other planets or asteroids, as well as in similarly demanding, harsh terrestrial settings. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Kobrick, Ryan L.; Klaus, David M.] Univ Colorado, Boulder, CO 80309 USA.
[Street, Kenneth W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Kobrick, RL (reprint author), Univ Colorado, 429 UCB, Boulder, CO 80309 USA.
EM Kobrick@Colorado.edu; Klaus@Colorado.edu; Kenneth.W.Street@nasa.gov
FU NASA [NNX07AR55H]; NASA Glenn Research Center
FX This research was supported by a NASA Graduate Student Researchers
Program (GSRP) grant (NNX07AR55H) provided by the Dust Management
Project, under the Exploration Technology Development Program. MATLAB
assistance was provided by Kevin Higdon, Ph.D. Candidate (UCB) and
Bradley W. Cheetham, Ph.D. Student (UCB). SEM work was conducted by
Prof. Sayed M. Khalil (Sohag University, Egypt) at the Nanomaterials
Characterization Facility, UCB. Test equipment and support were provided
by NASA Glenn Research Center. Additional support was provided by
BioServe Space Technologies (UCB) and the Achievement Rewards for
College Scientists (ARCS) Foundation, Inc.
NR 15
TC 4
Z9 4
U1 0
U2 2
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0043-1648
J9 WEAR
JI Wear
PD APR 4
PY 2011
VL 270
IS 9-10
BP 650
EP 657
DI 10.1016/j.wear.2011.01.026
PG 8
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 758AS
UT WOS:000290132500013
ER
PT J
AU Leer, K
Goetz, W
Chan, MA
Gorevan, S
Hansen, MF
Jensen, CL
Kletetschka, G
Kusack, A
Madsen, MB
AF Leer, Kristoffer
Goetz, Walter
Chan, Marjorie A.
Gorevan, Steven
Hansen, Mikkel Fougt
Jensen, Christian Lundmand
Kletetschka, Gunther
Kusack, Alastair
Madsen, Morten Bo
TI RAT magnet experiment on the Mars Exploration Rovers: Spirit and
Opportunity beyond sol 500
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MERIDIANI-PLANUM; DIAGENETIC HEMATITE; BURNS FORMATION; SOUTHERN UTAH;
FLUID-FLOW; USA
AB The Rock Abrasion Tool (RAT) magnet experiment on the Mars Exploration Rovers was designed to collect dust from rocks ground by the RAT of the two rovers on the surface of Mars. The dust collected on the magnets is now a mixture of dust from many grindings. Here the new data from the experiment are presented. The findings from Mars are furthermore compared to simulation experiments performed on Earth. New experiments with analog rocks that mainly contain hematite indicate the likely presence of a stronger magnetic phase besides hematite in the outcrop rock formations found on Meridiani Planum, a phase which was hitherto not detected by other measurements (such as Mossbauer) on these rocks.
C1 [Leer, Kristoffer; Jensen, Christian Lundmand; Madsen, Morten Bo] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Goetz, Walter] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Chan, Marjorie A.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA.
[Gorevan, Steven; Kusack, Alastair] Honeybee Robot, New York, NY 10001 USA.
[Hansen, Mikkel Fougt] Tech Univ Denmark, Dept Micro & Nanotechnol, DK-2800 Lyngby, Denmark.
[Kletetschka, Gunther] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Kletetschka, Gunther] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kletetschka, Gunther] Acad Sci Czech Republic, Inst Geol, Prague, Czech Republic.
RP Leer, K (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark.
EM kleer@kleer.dk
RI Kletetschka, Gunther/C-9996-2011; Hansen, Mikkel/A-3024-2012; Madsen,
Morten/D-2082-2011
OI Kletetschka, Gunther/0000-0002-0645-9037; Hansen,
Mikkel/0000-0003-3333-2856; Madsen, Morten/0000-0001-8909-5111
FU Danish Science Agency; Thomas B. Thrige's foundation; Danish
Electronics, Light, and Acoustics (DELTA) in Horsholm, Denmark; Honeybee
Robotics, New York
FX Danish participation in the MER missions was supported by the Danish
Science Agency, by Thomas B. Thrige's foundation, and by Danish
Electronics, Light, and Acoustics (DELTA) in Horsholm, Denmark. Honeybee
Robotics, New York, has been a very important player, and we thank
Honeybee for helping with simulation experiments. Tonci Balic-Zunic and
Anna Katerinopoulou from Institute of Geography and Geology, University
of Copenhagen, have been most helpful in acquisition and interpretation
of X-ray data. Furthermore, Mandy Bacon from the Niels Bohr Institute,
University of Copenhagen, has supported this project. We are indebted to
the scientists and engineers of the MER team for their continuous
support which made these experiments possible.
NR 25
TC 2
Z9 2
U1 0
U2 18
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 APR 2
PY 2011
VL 116
AR E00F18
DI 10.1029/2010JE003667
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 744HH
UT WOS:000289085000001
ER
PT J
AU Anderson, RL
Lo, MW
AF Anderson, Rodney L.
Lo, Martin W.
TI A Dynamical Systems Analysis of Resonant Flybys: Ballistic Case
SO JOURNAL OF THE ASTRONAUTICAL SCIENCES
LA English
DT Article
ID TRAJECTORY DESIGN; ORBITS; COMETS
AB In this analysis, resonant flybys were explored within the context of the circular restricted three-body problem using dynamical systems theory. The first step in this process involved the construction of a flyby trajectory continuously transiting between 3:4 and 5:6 resonances in the Jupiter-Europa circular restricted three-body problem. An examination of this trajectory revealed that it followed the invariant manifolds of resonant orbits during these transitions. It was discovered that these transitions occurred for specific energies where the invariant manifolds of the 3:4 and 5:6 resonant orbits were closely related. The potential of the information obtained from this analysis for use in mission design was demonstrated by developing resonance transition trajectories using resonant orbit homoclinic and heteroclinic connections.
C1 [Anderson, Rodney L.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
[Lo, Martin W.] CALTECH, Jet Prop Lab, High Capabil Comp & Modeling Grp, Pasadena, CA 91109 USA.
RP Anderson, RL (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
OI Anderson, Rodney/0000-0001-5336-2775
FU National Aeronautics and Space Administration; Jupiter Icy Moons Orbiter
mission design tool development task; JPL Institutional Computing and
Information Services; NASA Offices of Earth Science, Aeronautics, and
Space Science
FX The authors would like to thank Dr. George Born for his support of the
research and Dr. Bob Easton for his helpful discussions. This work was
conducted for the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. It was funded in part by the Jupiter Icy Moons Orbiter
mission design tool development task. The supercomputer used in this
investigation was provided by funding from JPL Institutional Computing
and Information Services and the NASA Offices of Earth Science,
Aeronautics, and Space Science.
NR 38
TC 10
Z9 10
U1 2
U2 4
PU AMER ASTRONAUTICAL SOC
PI SPRINGFIELD
PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA
SN 0021-9142
J9 J ASTRONAUT SCI
JI J. Astronaut. Sci.
PD APR-JUN
PY 2011
VL 58
IS 2
BP 167
EP 194
PG 28
WC Engineering, Aerospace
SC Engineering
GA 881CE
UT WOS:000299457300002
ER
PT J
AU Koshak, WJ
Solakewicz, RJ
AF Koshak, W. J.
Solakewicz, R. J.
TI Retrieving the Fraction of Ground Flashes from Satellite Lightning
Imager Data Using CONUS-Based Optical Statistics
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
AB A retrieval method is introduced for estimating the fraction of ground flashes in a set of N flashes observed from either a low earth-orbiting or geostationary satellite lightning imager. The methodology exploits the fact that mean optical characteristics of ground and cloud flashes differ, and hence a properly posed equation set for mean conditions of a set of N observed flashes can be mathematically inverted to estimate the ground flash fraction (and hence the cloud flash-to-ground flash ratio). Explicit analytic expressions for the retrieval errors are derived, and numerical tests of the retrieval method are provided to quantify retrieval accuracy. It has been found that the retrieval method works best when only one optimum optical parameter is used (the single-characteristic solution approach) rather than a mixture of optical parameters (the multiple-characteristic solution approach); that is, the suboptimum optical parameters in the mix degrade retrieval accuracy. Since the retrieval method uses conterminous United States (CONUS)-averaged values of the lightning optical measurements, retrieval errors tend to be smallest in geographical regions whose specific mean lightning optical measurements are closest to the CONUS mean values. The rms ground flash fraction retrieval errors for 52 widely distributed regions across CON US ranged from as low as 0.061 to 0.111, depending on the true ground flash fraction sought.
C1 [Koshak, W. J.] NASA Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA.
[Solakewicz, R. J.] Chicago State Univ, Chicago, IL USA.
RP Koshak, WJ (reprint author), NASA Marshall Space Flight Ctr, Earth Sci Off, VP61,Robert Cramer Res Hall,320 Sparkman Dr, Huntsville, AL 35805 USA.
EM william.koshak@nasa.gov
FU NOAA/NESDIS/STAR GOES-R Risk Reduction Program [NA07AA-NEG0284]; NASA
FX This research has been supported by the NOAA/NESDIS/STAR GOES-R Risk
Reduction Program under Space Act Agreement No. NA07AA-NEG0284 (Ms.
Ingrid Guch, Chief, NOAA/NESDIS/STAR Cooperative Research Programs
Division, Dr. Mark De Maria Chief, NOAA/NESDIS Regional and Mesoscale
Meteorology Branch, and Dr. Steven J. Goodman, Senior (Chief) Scientist,
GOES-R System Program), and by the Lightning Imaging Sensor (LIS)
project (Program Manager, Ramesh Kakar, NASA Headquarters) as part of
the NASA Earth Science Enterprise (ESE) Earth Observing system (EOS)
project. We would also like to express our thanks to the NASA
Postdoctoral Program (NPP) under which co-author Dr. Richard Solakiewicz
served during a portion of this research effort.
NR 4
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Z9 6
U1 1
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2011
VL 28
IS 4
BP 459
EP 473
DI 10.1175/2010JTECHA1408.1
PG 15
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 757AZ
UT WOS:000290057600002
ER
PT J
AU Koshak, WJ
AF Koshak, W. J.
TI A Mixed Exponential Distribution Model for Retrieving Ground Flash
Fraction from Satellite Lightning Imager Data
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
AB A Bayesian inversion method is introduced for retrieving the fraction of ground flashes in a set of flashes observed from a (low earth orbiting or geostationary) satellite lightning imager. The method employs a constrained mixed exponential distribution model to describe the lightning optical measurements. Because the method also retrieves certain population statistics of ground and cloud flash optical properties, the method can be applied to an arbitrary geographical region, including those regions where the lightning optical statistics either are not known or are difficult to obtain. The approach is tested by performing simulated retrievals, and retrieval error statistics are provided. A first-attempt retrieval of the global geographical distribution of ground flash fraction is obtained using the 5-yr Optical Transient Detector (OTD) dataset; the spatially averaged ground flash fraction over the global-scale domain studied was 0.151 with a standard deviation of 0.081. The ability to retrieve ground flash fraction has important benefits to the atmospheric chemistry community. For example, using the method to partition the existing OTD/Lightning Imaging Sensor (LIS) satellite global lightning climatology into separate ground and cloud flash climatologies would improve estimates of regional and global lightning nitrogen oxides (NO(x)) production; this, in turn, would improve both regional air quality and global chemistry/climate model predictions.
C1 NASA Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA.
RP Koshak, WJ (reprint author), NASA Marshall Space Flight Ctr, Earth Sci Off, 320 Sparkman Dr,VP61,Robert Cramer Res Hall, Huntsville, AL 35805 USA.
EM william.koshak@nasa.gov
FU NOAA/NESDIS/STAR GOES-R Risk Reduction Program [NA07AA-NEG0284]; NASA
Earth Science Enterprise (ESE) Earth Observing System (EOS)
FX This research has been supported by the NOAA/NESDIS/STAR GOES-R Risk
Reduction Program under Space Act Agreement NA07AA-NEG0284 [Ms. Ingrid
Guch, Chief, NOAA/NESDIS/STAR Cooperative Research Programs Division;
Dr. Mark De Maria, Chief, NOAA/NESDIS Regional and Mesoscale Meteorology
Branch; and Dr. Steven J. Goodman, Senior (Chief) Scientist, GOES-R
System Program], and by the Lightning Imaging Sensor (US) project
(Program Manager, Ramesh Kakar, NASA Headquarters) as part of the NASA
Earth Science Enterprise (ESE) Earth Observing System (EOS) project. The
author also thanks Dr. Richard Solakiewicz for his comments on a draft
version of this manuscript, and Dr. Harold Peterson (NASA Postdoctoral
Program) for his clerical help in finding some of the references cited
here.
NR 14
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U1 0
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 APR
PY 2011
VL 28
IS 4
BP 475
EP 492
DI 10.1175/2010JTECHA1438.1
PG 18
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 757AZ
UT WOS:000290057600003
ER
PT J
AU Shindell, D
Faluvegi, G
Walsh, M
Anenberg, SC
Van Dingenen, R
Muller, NZ
Austin, J
Koch, D
Milly, G
AF Shindell, Drew
Faluvegi, Greg
Walsh, Michael
Anenberg, Susan C.
Van Dingenen, Rita
Muller, Nicholas Z.
Austin, Jeff
Koch, Dorothy
Milly, George
TI Climate, health, agricultural and economic impacts of tighter
vehicle-emission standards
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID AIR-POLLUTION; OZONE; STRATEGIES; MORTALITY; BENEFITS; SECTORS; ROAD
AB Non-CO2 air pollutants from motor vehicles have traditionally been controlled to protect air quality and health, but also affect climate. We use global composition-climate modelling to examine the integrated impacts of adopting stringent European on-road vehicle-emission standards for these pollutants in 2015 in many developing countries. Relative to no extra controls, the tight standards lead to annual benefits in 2030 and beyond of 120,000-280,000 avoided premature air pollution-related deaths, 6.1-19.7 million metric tons of avoided ozone-related yield losses of major food crops, $1.50.6-2.4 trillion avoided health damage and $US1.1-4.3 billion avoided agricultural damage, and mitigation of 0.20 (+0.14/-0.17)degrees C of Northern Hemisphere extratropical warming during 2040-2070. Tighter vehicle-emission standards are thus extremely likely to mitigate short-term climate change in most cases, in addition to providing large improvements in human health and food security. These standards will not reduce CO2 emissions, however, which is required to mitigate long-term climate change.
C1 [Shindell, Drew; Faluvegi, Greg; Koch, Dorothy; Milly, George] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Shindell, Drew; Faluvegi, Greg; Koch, Dorothy; Milly, George] Columbia Univ, Columbia Earth Inst, New York, NY 10025 USA.
[Walsh, Michael] Int Council Clean Transportat, San Francisco, CA 94104 USA.
[Anenberg, Susan C.] US EPA, Res Triangle Pk, NC 27711 USA.
[Anenberg, Susan C.] Univ N Carolina, Dept Environm Sci & Engn, Chapel Hill, NC 27599 USA.
[Van Dingenen, Rita] Inst Environm & Sustainabil, European Commiss, Joint Res Ctr, I-21027 Ispra, Italy.
[Muller, Nicholas Z.] Middlebury Coll, Dept Econ, Middlebury, VT 05753 USA.
[Austin, Jeff] Calif Air Resources Board, Sacramento, CA 95814 USA.
RP Shindell, D (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM drew.t.shindell@nasa.gov
RI Shindell, Drew/D-4636-2012
FU NASA; ClimateWorks Foundation; California Air Resources Board
FX We thank the NASA Applied Sciences program, the ClimateWorks Foundation
and the California Air Resources Board for supporting this work. We also
thank T. Bond for gridding the emissions, M. Brauer for providing the
PM2.5-measurement database, J. West for assistance with the population
projection, B. Croes and D. Luo at GARB for their assistance and the
UNEP/WMO Integrated Assessment of Black Carbon and Tropospheric Ozone
team for discussions. Conclusions expressed in this article are the
authors and do not necessarily represent those of their employers.
NR 38
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U1 3
U2 34
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD APR
PY 2011
VL 1
IS 1
BP 59
EP 66
DI 10.1038/NCLIMATE1066
PG 8
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 805HS
UT WOS:000293718100025
ER
PT J
AU Johnson, PV
Hodyss, R
Tang, KQ
Brinckerhoff, WB
Smith, RD
AF Johnson, Paul V.
Hodyss, Robert
Tang, Keqi
Brinckerhoff, William B.
Smith, Richard D.
TI The laser ablation ion funnel: Sampling for in situ mass spectrometry on
Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Ion funnel; Laser ablation; Mars; Mass spectrometry
ID INTERFACE; PRESSURE; PERFORMANCE; TRANSPORT; DESIGN; SPACE
AB A considerable investment has been made by NASA and other space agencies to develop instrumentation suitable for in situ analytical investigation of extra terrestrial bodies including various mass spectrometers (time-of-flight, quadrupole ion trap, quadrupole mass filters, etc.). However, the front-end sample handling that is needed to collect and prepare samples for interrogation by such instrumentation remains underdeveloped. Here we describe a novel approach tailored to the exploration of Mars where ions are created in the ambient atmosphere via laser ablation and then efficiently transported into a mass spectrometer for in situ analysis using an electrodynamic ion funnel. This concept would enable elemental and isotopic analysis of geological samples with the analysis of desorbed organic material a possibility as well. Such an instrument would be suitable for inclusion on all potential missions currently being considered such as the Mid-Range Rover, the Astrobiology Field Laboratory, and Mars Sample Return (i.e., as a sample pre-selection triage instrument), among others. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Johnson, Paul V.; Hodyss, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
[Tang, Keqi; Smith, Richard D.] Pacific NW Natl Lab, Environm Mol Sci Lab, Richland, WA 99352 USA.
[Tang, Keqi; Smith, Richard D.] Pacific NW Natl Lab, Div Biol Sci, Richland, WA 99352 USA.
[Brinckerhoff, William B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Johnson, PV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
EM Paul.V.Johnson@jpl.nasa.gov
RI Smith, Richard/J-3664-2012; Brinckerhoff, William/F-3453-2012; Johnson,
Paul/D-4001-2009
OI Smith, Richard/0000-0002-2381-2349; Brinckerhoff,
William/0000-0001-5121-2634; Johnson, Paul/0000-0002-0186-8456
FU National Aeronautics and Space Administration (NASA); DOE [DE-AC05-76RLO
1830]; NASA; JPL
FX This work was performed at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration (NASA) and at the Environmental
Molecular Sciences Laboratory, a US DOE national scientific user
facility located at the Pacific Northwest National Laboratory (PNNL) in
Richland, Washington. PNNL is a multiprogram national laboratory
operated by Battelle for the DOE under Contract no. DE-AC05-76RLO 1830.
Funding from NASA's Planetary Instrument Definition and Development
program and the JPL Director's Research and Development Fund is
gratefully acknowledged.
NR 27
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U1 5
U2 27
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 APR
PY 2011
VL 59
IS 5-6
BP 387
EP 393
DI 10.1016/j.pss.2011.01.004
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737PT
UT WOS:000288581400003
ER
PT J
AU Cordiner, MA
Charnley, SB
Buckle, JV
Walsh, C
Millar, TJ
AF Cordiner, M. A.
Charnley, S. B.
Buckle, J. V.
Walsh, C.
Millar, T. J.
TI DISCOVERY OF INTERSTELLAR ANIONS IN CEPHEUS AND AURIGA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; stars:
formation
ID MASS PROTOSTAR IRAS-04368+2557; CARBON-CHAIN MOLECULES; STAR-FORMING
REGIONS; GAS GRAIN PROCESSES; DARK CLOUDS; ASTRONOMICAL IDENTIFICATION;
INITIAL CONDITIONS; CHEMICAL-MODELS; DENSE CORES; L1527
AB We report the detection of microwave emission lines from the hydrocarbon anion C6H- and its parent neutral C6H in the star-forming region L1251A (in Cepheus), and the pre-stellar core L1512 (in Auriga). The carbon-chain-bearing species C4H, HC3N, HC5N, HC7N, and C3S are also detected in large abundances. The observations of L1251A constitute the first detections of anions and long-chain polyynes and cyanopolyynes (with more than five carbon atoms) in the Cepheus Flare star-forming region, and the first detection of anions in the vicinity of a protostar outside of the Taurus molecular cloud complex, indicating a possible wider importance for anions in the chemistry of star formation. Rotational excitation temperatures have been derived from the HC3N hyperfine structure lines and are found to be 6.2 K for L1251A and 8.7 K for L1512. The anion-to-neutral ratios are 3.6% and 4.1%, respectively, which are within the range of values previously observed in the interstellar medium, and suggest a relative uniformity in the processes governing anion abundances in different dense interstellar clouds. This research contributes toward the growing body of evidence that carbon chain anions are relatively abundant in interstellar clouds throughout the Galaxy, but especially in the regions of relatively high density and high depletion surrounding pre-stellar cores and young, embedded protostars.
C1 [Cordiner, M. A.; Charnley, S. B.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
[Cordiner, M. A.; Charnley, S. B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Buckle, J. V.] Univ Cambridge, Cavendish Astrophys Grp, Cambridge CB3 0HE, England.
[Buckle, J. V.] Univ Cambridge, Kavli Inst Cosmol, Inst Astron, Cambridge CB3 0HE, England.
[Walsh, C.; Millar, T. J.] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
RP Cordiner, MA (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM martin.cordiner@nasa.gov
RI Charnley, Steven/C-9538-2012;
OI Millar, Tom/0000-0001-5178-3656
FU NASA; Goddard Center for Astrobiology; STFC
FX This research was supported by the NASA Exobiology Program and the
Goddard Center for Astrobiology. Astrophysics at QUB is supported by a
grant from STFC.
NR 50
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U1 1
U2 10
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 APR 1
PY 2011
VL 730
IS 2
AR L18
DI 10.1088/2041-8205/730/2/L18
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797KK
UT WOS:000293125600006
ER
PT J
AU Gilli, R
Su, J
Norman, C
Vignali, C
Comastri, A
Tozzi, P
Rosati, P
Stiavelli, M
Brandt, WN
Xue, YQ
Luo, B
Castellano, M
Fontana, A
Fiore, F
Mainieri, V
Ptak, A
AF Gilli, R.
Su, J.
Norman, C.
Vignali, C.
Comastri, A.
Tozzi, P.
Rosati, P.
Stiavelli, M.
Brandt, W. N.
Xue, Y. Q.
Luo, B.
Castellano, M.
Fontana, A.
Fiore, F.
Mainieri, V.
Ptak, A.
TI A COMPTON-THICK ACTIVE GALACTIC NUCLEUS AT z similar to 5 IN THE 4 Ms
CHANDRA DEEP FIELD SOUTH
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: high-redshift; X-rays: galaxies
ID STAR-FORMATION RATE; BLACK-HOLES; SUBMILLIMETER GALAXY; INFRARED
GALAXIES; HELLAS2XMM SURVEY; SOURCE CATALOGS; SPACE DENSITY; OBSCURED
AGN; STELLAR MASS; RAY
AB We report the discovery of a Compton-thick active galactic nucleus (AGN) at z = 4.76 in the 4 Ms Chandra Deep Field South. This object was selected as a V-band dropout in HST/ACS images and previously recognized as an AGN from optical spectroscopy. The 4Ms Chandra observations show a significant (similar to 4.2 sigma) X-ray detection at the V-band dropout position. The X-ray source displays a hardness ratio of HR = 0.23 +/- 0.24, which, for a source at z similar to 5, is highly suggestive of Compton-thick absorption. The source X-ray spectrum is seen above the background level in the energy range of similar to 0.9-4 keV, i.e., in the rest-frame energy range of similar to 5-23 keV. When fixing the photon index to Gamma = 1.8, the measured column density is N-H = 1.4(-0.5)(+0.9) x 10(24) cm(-2), which is Compton thick. To our knowledge, this is the most distant heavily obscured AGN, confirmed by X-ray spectral analysis, discovered so far. The intrinsic (de-absorbed), rest-frame luminosity in the 2-10 keV band is similar to 2.5 x 10(44) erg s(-1), which places this object among type-2 quasars. The spectral energy distribution shows that massive star formation is associated with obscured black hole (BH) accretion. This system may have then been caught during a major coeval episode of BH and stellar mass assembly at early times. The measure of the number density of heavily obscured AGN at high redshifts will be crucial to reconstructing the BH/galaxy evolution history from the beginning.
C1 [Gilli, R.; Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Su, J.; Norman, C.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Norman, C.; Stiavelli, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Tozzi, P.] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy.
[Rosati, P.; Mainieri, V.] European So Observ, D-85748 Garching, Germany.
[Brandt, W. N.; Xue, Y. Q.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Brandt, W. N.; Xue, Y. Q.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Castellano, M.; Fontana, A.; Fiore, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gilli, R (reprint author), INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
EM roberto.gilli@oabo.inaf.it
RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015;
OI Vignali, Cristian/0000-0002-8853-9611; Brandt,
William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970;
Gilli, Roberto/0000-0001-8121-6177; Castellano,
Marco/0000-0001-9875-8263; fontana, adriano/0000-0003-3820-2823; Fiore,
Fabrizio/0000-0002-4031-4157
FU Italian Space Agency (ASI) under the ASI-INAF [I/009/10/0, I/088/06/0];
NASA [SP1-12007A, NNX10AC99G]; Chandra archival grant [SP89004X]; DFG
cluster of excellence Origin and Structure of the Universe
FX We acknowledge the following supporting agencies and grants: Italian
Space Agency (ASI) under the ASI-INAF contracts I/009/10/0 and
I/088/06/0 (R. G., C. V., A. C.); NASA through CXC grant SP1-12007A and
ADP grant NNX10AC99G (W.N.B., Y.Q.X., B. L.); Chandra archival grant
SP89004X (A. P., R. G.); DFG cluster of excellence Origin and Structure
of the Universe (P. R.). We thank the referee for a constructive report
and N. Miller and M. Mignoli for useful discussions. R. G. gratefully
acknowledges hospitality by the Johns Hopkins University where this work
started.
NR 51
TC 31
Z9 31
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 APR 1
PY 2011
VL 730
IS 2
AR L28
DI 10.1088/2041-8205/730/2/L28
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797KK
UT WOS:000293125600016
ER
PT J
AU Morales, FY
Rieke, GH
Werner, MW
Bryden, G
Stapelfeldt, KR
Su, KYL
AF Morales, Farisa Y.
Rieke, G. H.
Werner, M. W.
Bryden, G.
Stapelfeldt, K. R.
Su, K. Y. L.
TI COMMON WARM DUST TEMPERATURES AROUND MAIN-SEQUENCE STARS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; infrared: stars; interplanetary medium
ID SPITZER-SPACE-TELESCOPE; SUN-LIKE STARS; TURBULENT PROTOPLANETARY DISKS;
DEBRIS DISKS; SNOW LINE; ASTEROID BELT; HR 8799; EMISSION; POPULATION;
COLLISIONS
AB We compare the properties of warm dust emission from a sample of main-sequence A-type stars (B8-A7) to those of dust around solar-type stars (F5-K0) with similar Spitzer Space Telescope Infrared Spectrograph/MIPS data and similar ages. Both samples include stars with sources with infrared spectral energy distributions that show evidence of multiple components. Over the range of stellar types considered, we obtain nearly the same characteristic dust temperatures (similar to 190 K and similar to 60 K for the inner and outer dust components, respectively)-slightly above the ice evaporation temperature for the inner belts. The warm inner dust temperature is readily explained if populations of small grains are being released by sublimation of ice from icy planetesimals. Evaporation of low-eccentricity icy bodies at similar to 150 K can deposit particles into an inner/warm belt, where the small grains are heated to T-dust similar to 190 K. Alternatively, enhanced collisional processing of an asteroid belt-like system of parent planetesimals just interior to the snow line may account for the observed uniformity in dust temperature. The similarity in temperature of the warmer dust across our B8-K0 stellar sample strongly suggests that dust-producing planetesimals are not found at similar radial locations around all stars, but that dust production is favored at a characteristic temperature horizon.
C1 [Morales, Farisa Y.; Werner, M. W.; Bryden, G.; Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morales, Farisa Y.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
[Rieke, G. H.; Su, K. Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bryden, G.] CALTECH, NExScI, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Morales, FY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Farisa@jpl.nasa.gov
RI Stapelfeldt, Karl/D-2721-2012;
OI Su, Kate/0000-0002-3532-5580
FU NASA [1407]
FX We thank Paul Weissman and Neal Turner (JPL) for their helpful comments
and stimulating discussions, and the referee for the careful reading and
detailed comments. This work is based on observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under NASA contract
1407.
NR 40
TC 59
Z9 59
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 1
PY 2011
VL 730
IS 2
AR L29
DI 10.1088/0004-637X/730/2/L29
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797KK
UT WOS:000293125600017
ER
PT J
AU Raga, AC
Noriega-Crespo, A
Lora, V
Stapelfeldt, KR
Carey, SJ
AF Raga, A. C.
Noriega-Crespo, A.
Lora, V.
Stapelfeldt, K. R.
Carey, S. J.
TI THE JET/COUNTERJET INFRARED SYMMETRY OF HH 34 AND THE SIZE OF THE JET
FORMATION REGION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; Herbig-Haro objects; infrared: ISM; ISM:
individual objects (HH 34); ISM: jets and outflows; stars: formation
ID SPITZER-SPACE-TELESCOPE; BOW SHOCK; HH-34 JET; IMAGES; KINEMATICS;
EVOLUTION; EMISSION; OUTFLOWS; COMPLEX; SYSTEM
AB We present new Spitzer IRAC images of the HH 34 outflow. These are the first images that detect both the knots along the southern jet and the northern counterjet (the counterjet knots were only detected previously in a long-slit spectrum). This result removes the problem of the apparent coexistence of a large-scale symmetry (at distances of up to similar to 1 pc) and a complete lack of symmetry close to the source (at distances of similar to 10(17) cm) for this outflow. We present a quantitative evaluation of the newly found symmetry between the HH 34 jet and counterjet, and show that the observed degree of symmetry implies that the jet production region has a characteristic size < 2.8 AU. This is the strongest constraint yet derived for the size of the region in which HH jets are produced.
C1 [Raga, A. C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
[Noriega-Crespo, A.; Carey, S. J.] CALTECH, SPITZER Sci Ctr, Pasadena, CA 91125 USA.
[Lora, V.] Univ Heidelberg, Astron Rechen Inst Zentrum Astron, D-69120 Heidelberg, Germany.
[Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Raga, AC (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Ap 70-543, Mexico City 04510, DF, Mexico.
FU NASA [1407]; CONACyT [61547, 101356, 101975]
FX This work is based in part on observations made with the Spitzer Space
Telescope which is operated by the Jet Propulsion Laboratory, California
Institute of Technology under NASA contract 1407. The work of A. R. and
V. L. was supported by the CONACyT grants 61547, 101356, and 101975.
NR 30
TC 11
Z9 11
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 1
PY 2011
VL 730
IS 2
AR L17
DI 10.1088/2041-8205/730/2/L17
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797KK
UT WOS:000293125600005
ER
PT J
AU Halkides, D
Lee, T
AF Halkides, Daria
Lee, Tong
TI Mechanisms controlling seasonal mixed layer temperature and salinity in
the Southwestern Tropical Indian Ocean
SO DYNAMICS OF ATMOSPHERES AND OCEANS
LA English
DT Article
DE Indian Ocean; Thermocline ridge; Mixed layer budgets
ID SHALLOW-WATER SIMULATIONS; SEA-LEVEL VARIATIONS; INTERANNUAL
VARIABILITY; INTRASEASONAL VARIABILITY; STATISTICAL PREDICTION;
INDONESIAN THROUGHFLOW; CIRCULATION MODEL; SURFACE CURRENTS;
HEAT-TRANSPORT; PACIFIC-OCEAN
AB We use a heat-and salt-conserving ocean state estimation product to study the seasonal cycles of the mixed layer (ML) temperature (MLT) and salinity (MIS) balances over the southwestern tropical Indian Ocean (SWTIO) thermocline ridge (STR; 50 degrees-75 degrees E, 12 degrees-5 degrees S). For seasonal MLT, surface heat flux and ocean processes are both important. They tend to re-enforce each other during peak cooling (May-June) and warming (November) periods, but not during transition periods. The dominant ocean process is wind-driven vertical mixing. It is modulated by the variable strength of the monsoon winds (which affect the vertical diffusivity), and to a lesser extent by variability of thermocline depth (which influences the vertical stratification across the ML base). For example, thermocline shoaling in April-July alters the vertical stratification near the ML base; thus, when the monsoon winds heighten (June-September) and the vertical diffusivity increases (deepening the ML base), relatively cool subsurface water is near the ML base and easily incorporated into the ML by vertical mixing. However, vertical advection as a direct response to thermocline shoaling has little affect on MLT. This explains why MLT and thermocline depth are not positively correlated here on the seasonal timescale (as they are on the interannual timescale). Meridional advection associated with Ekman transport driven by the monsoon winds plays a secondary role. Seasonal MLS, however, is dominated by meridional advection. Vertical process effects on MLS are small, due to a weak salinity gradient near the ML base throughout the year. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Halkides, Daria] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90024 USA.
[Halkides, Daria; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Halkides, D (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90024 USA.
EM halkides@jpl.nasa.gov
FU NASA; PO.DAAC (http://podaac.jpl.nasa.gov)
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. Support by
PO.DAAC (http://podaac.jpl.nasa.gov) is acknowledged. The 1992-2002 mean
ocean dynamic topography data was obtained from Nikolai Maximenko (IPRC)
and Peter Niiler (SIO;
http://apdrc.soest.hawaii.edu/projects/DOT/index.html).
NR 64
TC 11
Z9 12
U1 1
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0265
J9 DYNAM ATMOS OCEANS
JI Dyn. Atmos. Oceans
PD APR
PY 2011
VL 51
IS 3
BP 77
EP 93
DI 10.1016/j.dynatmoce.2011.03.002
PG 17
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences;
Oceanography
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences;
Oceanography
GA 795AV
UT WOS:000292944800002
ER
PT J
AU Hagler, P
Johnson, RW
Chen, LY
AF Hagler, Ping
Johnson, R. Wayne
Chen, Liang-Yu
TI SiC Die Attach Metallurgy and Processes for Applications up to 500
degrees C
SO IEEE TRANSACTIONS ON COMPONENTS PACKAGING AND MANUFACTURING TECHNOLOGY
LA English
DT Article
DE Die attach; die metallization; high temperature; liquid transient phase
bonding
ID LOW-TEMPERATURE
AB The challenges of packaging SiC-based electronics for high-temperature applications include their high operating temperatures, wide thermal cycle ranges, and, sometimes, high currents and high voltages. As a result, the selection of metallurgy for high-temperature SiC die attach is crucial to a successful package design, which involves chip metallization, substrate metallization, and die attach alloy. This paper examines off-eutectic Au-Sn as the die attach alloy with a PtAu thick film metallization on AlN substrates. A pure Au thick film layer was printed over the PtAu thick film layer. AlN substrates metalized with refractory MoMn and electroplated Ni/Au were also used. Two different die attach approaches have been investigated, using Sn-Au-Sn off-eutectic thick foil and limited-volume eutectic AuSn (80/20 wt.%) preform. The SiC backside metallizations evaluated were Ti/TaSi(2)/Pt/Au and Cr/NiCr/Au. Die shear tests were performed after aging at 500 degrees C and after thermal cycling. The shear test results and failure surface analysis are discussed.
C1 [Hagler, Ping] Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA.
[Johnson, R. Wayne] Auburn Univ, Dept Elect & Commun Engn, Auburn, AL 36849 USA.
[Chen, Liang-Yu] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
RP Hagler, P (reprint author), Missile Def Agcy, Dept Def, Washington, DC 20301 USA.
EM ping.hagler@hotmail.com; john-son@eng.auburn.edu;
liangyu.chen-1@nasa.gov
FU National Aeronautics and Space Administration (NASA) [NNC07ZA11A]
FX This work was supported in part by the Integrated Vehicle Health
Management Project of National Aeronautics and Space Administration
(NASA) Aviation Safety Program under the NASA Research Announcement
Grant NNC07ZA11A monitored by G. W. Hunter at the NASA Glenn Research
Center. Recommended for publication by Associate Editor I. Fidan upon
evaluation of reviewers' comments.
NR 14
TC 11
Z9 11
U1 0
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-3950
J9 IEEE T COMP PACK MAN
JI IEEE Trans. Compon. Pack. Manuf. Technol.
PD APR
PY 2011
VL 1
IS 4
BP 630
EP 639
DI 10.1109/TCPMT.2011.2106160
PG 10
WC Engineering, Manufacturing; Engineering, Electrical & Electronic;
Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 793MP
UT WOS:000292827500019
ER
PT J
AU Sun, J
Choi, KK
Jhabvala, MD
Jhabvala, C
AF Sun, Jason
Choi, Kwong-Kit
Jhabvala, Merzy D.
Jhabvala, Christine
TI Advanced substrate thinning process for GaAs-based devices
SO JOURNAL OF MICRO-NANOLITHOGRAPHY MEMS AND MOEMS
LA English
DT Article
DE inductively coupled plasma selective etching; corrugated quantum well
infrared photodetector focal plane arrays; GaAs substrate thinning
ID ALGAAS; ETCH; PLASMAS; LAYERS; DAMAGE
AB We developed an optimized substrate removal process for GaAs-based opto-electronic devices by establishing a reliable two-step process. In this process, the substrate is first thinned by mechanical lapping and then followed by selective high density plasma etching. The adopted inductively coupled plasma etching, having an optimized boron trichloride (BCl3)/sulfur hexafluoride (SF6)/argon composition, shows a nearly infinite etching selectivity for the GaAs substrate over the aluminum gallium arsenide (AlxGa1-xAs) etch-stop layer. The surface of the die is perfectly smooth and mirror-like after processing. In addition to its simplicity, the process is also highly reproducible and shows no damage to the underlying detector material. (C) 2011 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI:10.1117/1.3580755]
C1 [Sun, Jason; Choi, Kwong-Kit] USA, Res Lab, Adelphi, MD 20783 USA.
[Jhabvala, Merzy D.; Jhabvala, Christine] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sun, J (reprint author), USA, Res Lab, Adelphi, MD 20783 USA.
EM jason.sun@arl.army.mil
RI Choi, Kwong-Kit/K-9205-2013
NR 11
TC 5
Z9 5
U1 0
U2 3
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1932-5150
J9 J MICRO-NANOLITH MEM
JI J. Micro-Nanolithogr. MEMS MOEMS
PD APR-JUN
PY 2011
VL 10
IS 2
AR 023004
DI 10.1117/1.3580755
PG 4
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Materials Science, Multidisciplinary; Optics
SC Engineering; Science & Technology - Other Topics; Materials Science;
Optics
GA 787JU
UT WOS:000292373200006
ER
PT J
AU Wahlgren, GM
AF Wahlgren, Glenn M.
TI Atomic data for stellar astrophysics: from the UV to the IR
SO CANADIAN JOURNAL OF PHYSICS
LA English
DT Article; Proceedings Paper
CT 10th International Colloquium on AtomicSpectroscopy and Oscillator
Strengths for Astrophysical andLaboratory Plasmas (ASOS)
CY AUG 03-07, 2010
CL Berkeley, CA
ID CHEMICALLY PECULIAR STAR; FINE-STRUCTURE LINES;
TRANSITION-PROBABILITIES; OSCILLATOR-STRENGTHS; ENERGY-LEVELS;
WAVELENGTH DETERMINATIONS; SPECTRAL CLASSIFICATION; RADIATIVE LIFETIMES;
EMISSION-LINES; COOL STARS
AB The study of stars and stellar evolution relies heavily on the analysis of stellar spectra. The need for atomic line data from the ultraviolet (UV) to the infrared (IR) regions is greater now than ever. In the past twenty years, the time since the launch of the Hubble Space Telescope, great progress has been made in acquiring atomic data for UV transitions. The optical wavelength region, now expanded by progress in detector technology, continues to provide motivation for new atomic data. In addition, investments in new instrumentation for ground-based and space observatories has lead to the availability of high-quality spectra at IR wavelengths, where the need for atomic data is most critical. In this review, examples are provided of the progress made in generating atomic data for stellar studies, with a look to the future for addressing the accuracy and completeness of atomic data for anticipated needs.
C1 [Wahlgren, Glenn M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wahlgren, Glenn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wahlgren, GM (reprint author), NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
EM glenn.m.wahlgren@nasa.gov
FU NASA [NNG06GJ29G]
FX The author acknowledges support from NASA grant NNG06GJ29G.
NR 66
TC 3
Z9 3
U1 1
U2 4
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA
SN 0008-4204
EI 1208-6045
J9 CAN J PHYS
JI Can. J. Phys.
PD APR
PY 2011
VL 89
IS 4
BP 345
EP 356
DI 10.1139/P10-125
PG 12
WC Physics, Multidisciplinary
SC Physics
GA 775QA
UT WOS:000291475700005
ER
PT J
AU Sterling, NC
Witthoeft, MC
Esteves, DA
Bilodeau, RC
Kilcoyne, ALD
Red, EC
Phaneuf, RA
Alna'Washi, G
Aguilar, A
AF Sterling, N. C.
Witthoeft, M. C.
Esteves, D. A.
Bilodeau, R. C.
Kilcoyne, A. L. D.
Red, E. C.
Phaneuf, R. A.
Alna'Washi, G.
Aguilar, A.
TI New atomic data for trans-iron elements and their application to
abundance determinations in planetary nebulae
SO CANADIAN JOURNAL OF PHYSICS
LA English
DT Article; Proceedings Paper
CT 10th International Colloquium on AtomicSpectroscopy and Oscillator
Strengths for Astrophysical andLaboratory Plasmas (ASOS)
CY AUG 03-07, 2010
CL Berkeley, CA
ID GIANT BRANCH STARS; NEUTRON-CAPTURE ELEMENTS; EFFECTIVE COLLISION
STRENGTHS; S-PROCESS; CHARGE-TRANSFER; DIELECTRONIC RECOMBINATION;
FORBIDDEN TRANSITIONS; CROSS-SECTIONS; MASSIVE STARS; CONFIGURATIONS
AB Investigations of neutron(n)-capture element nucleosynthesis and chemical evolution have largely been based on stellar spectroscopy. However, the recent detection of these elements in several planetary nebulae (PNe) indicates that nebular spectroscopy is a promising new tool for such studies. In PNe, n-capture element abundance determinations reveal details of s-process nucleosynthesis and convective mixing in evolved low-mass stars, as well as the chemical evolution of elements that cannot be detected in stellar spectra. Only one or two ions of a given trans-iron element can typically be detected in individual nebulae. Elemental abundance determinations thus require corrections for the abundances of unobserved ions. Such corrections rely on the availability of atomic data for processes that control the ionization equilibrium of nebulae (e. g., photoionization cross sections and rate coefficients for various recombination processes). Until recently, these data were unknown for virtually all n-capture element ions. For the first six ions of Se, Kr, and Xe - the three most widely detected n-capture elements in PNe we are calculating photoionization cross sections and radiative and dielectronic recombination rate coefficients using the multi-configuration Breit-Pauli atomic structure code AUTOSTRUCTURE. Charge transfer rate coefficients are being determined with a multichannel Landau-Zener code. To calibrate these calculations, we have measured absolute photoionization cross sections of Se and Xe ions at the Advanced Light Source synchrotron radiation facility. These atomic data can be incorporated into photoionization codes, which we will use to derive ionization corrections (hence abundances) for Se, Kr, and Xe in ionized nebulae. Using Monte Carlo simulations, we will investigate the effects of atomic data uncertainties on the derived abundances, illuminating the systems and atomic processes that require further analysis. These results are critical for honing nebular spectroscopy into a more effective tool for investigating the production and chemical evolution of trans-iron elements in the Universe.
C1 [Sterling, N. C.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Witthoeft, M. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Esteves, D. A.; Phaneuf, R. A.; Alna'Washi, G.] Univ Nevada, Dept Phys, Reno, NV 89557 USA.
[Bilodeau, R. C.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Kilcoyne, A. L. D.; Red, E. C.; Aguilar, A.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
RP Sterling, NC (reprint author), Michigan State Univ, Dept Phys & Astron, 3248 Biomed Phys Sci, E Lansing, MI 48824 USA.
EM sterling@pa.msu.edu
RI Kilcoyne, David/I-1465-2013;
OI Bilodeau, Rene/0000-0001-8607-2328
FU Office of Science, Office of Basic Energy Sciences, of the US Department
of Energy [DE-AC02-05CH11231, DE-AC03-76SF-00098, DE-FG02-03ER15424];
National Science Foundation [AST-0901432]; NASA [06-APRA206-0049]; NASA
Goddard Space Flight Center [NNX08AJ96G]
FX We acknowledge support by the Director, Office of Science, Office of
Basic Energy Sciences, of the US Department of Energy under contracts
DE-AC02-05CH11231, DE-AC03-76SF-00098, and grant DE-FG02-03ER15424. N.
C. Sterling acknowledges support from an National Science Foundation
Astronomy and Astrophysics Postdoctoral Fellowship under award
AST-0901432 and from NASA grant 06-APRA206-0049. D. Esteves acknowledges
support from grant NNX08AJ96G with NASA Goddard Space Flight Center and
the Doctoral Fellowship Program at the Advanced Light Source. We thank
N. R. Badnell for many enlightening discussions regarding AUTOSTRUCTURE,
and P. Stancil for helpful discussions and providing a code for our CT
calculations.
NR 57
TC 7
Z9 7
U1 0
U2 7
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA
SN 0008-4204
EI 1208-6045
J9 CAN J PHYS
JI Can. J. Phys.
PD APR
PY 2011
VL 89
IS 4
BP 379
EP 385
DI 10.1139/P10-105
PG 7
WC Physics, Multidisciplinary
SC Physics
GA 775QA
UT WOS:000291475700009
ER
PT J
AU Forth, KE
Fiedler, MJ
Paloski, WH
AF Forth, Katharine E.
Fiedler, Matthew J.
Paloski, William H.
TI Estimating functional stability boundaries for bipedal stance
SO GAIT & POSTURE
LA English
DT Article
DE Balance control; Stability limits; Falls; Time-to-boundary; Stability
margin
ID TIME; POSTUROGRAPHY; CONTACT; LIMITS; AGE
AB We propose a technique to estimate functional limits of stability (LOS) during bipedal stance using a controlled, low speed, voluntary leaning protocol requiring feet to remain in contact with the ground. LOS are estimated from ellipses fit to center-of-mass position data obtained during the leaning protocol. The LOS of nine healthy subjects were found to be 20-59% closer to the center of stance than the more frequently used anatomical boundaries and were reduced by closing the eyes. We conclude that functional stability boundaries should be used when the outcome measure is related to fall risk. Published by Elsevier B.V.
C1 [Paloski, William H.] Univ Houston, Ctr Neuromotor & Biomech Res, Houston, TX 77204 USA.
[Forth, Katharine E.] Univ Space Res Assoc, Houston, TX USA.
[Fiedler, Matthew J.] Wyle Integrated Sci & Engn Grp, Houston, TX USA.
[Paloski, William H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Paloski, WH (reprint author), Univ Houston, Ctr Neuromotor & Biomech Res, 3855 Holman St,Garrison 104, Houston, TX 77204 USA.
EM whpaloski@uh.edu
NR 10
TC 6
Z9 6
U1 0
U2 7
PU ELSEVIER IRELAND LTD
PI CLARE
PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000,
IRELAND
SN 0966-6362
J9 GAIT POSTURE
JI Gait Posture
PD APR
PY 2011
VL 33
IS 4
BP 715
EP 717
DI 10.1016/j.gaitpost.2010.12.024
PG 3
WC Neurosciences; Orthopedics; Sport Sciences
SC Neurosciences & Neurology; Orthopedics; Sport Sciences
GA 771EI
UT WOS:000291139600036
PM 21277211
ER
PT J
AU Barker, HW
Jerg, MP
Wehr, T
Kato, S
Donovan, DP
Hogan, RJ
AF Barker, H. W.
Jerg, M. P.
Wehr, T.
Kato, S.
Donovan, D. P.
Hogan, R. J.
TI A 3D cloud-construction algorithm for the EarthCARE satellite mission
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE cloud; radiative transfer; satellite; EarthCARE
ID ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM
INSTRUMENT; ACCURATE PARAMETERIZATION; OPTICAL-PROPERTIES; UNRESOLVED
CLOUDS; TERRA SATELLITE; CLIMATE MODELS; CIRRUS CLOUDS; WATER CLOUDS
AB This article presents and assesses an algorithm that constructs 3D distributions of cloud from passive satellite imagery and collocated 2D nadir profiles of cloud properties inferred synergistically from lidar, cloud radar and imager data. It effectively widens the active-passive retrieved cross-section (RXS) of cloud properties, thereby enabling computation of radiative fluxes and radiances that can be compared with measured values in an attempt to perform radiative closure experiments that aim to assess the RXS. For this introductory study, A-train data were used to verify the scene-construction algorithm and only 1D radiative transfer calculations were performed.
The construction algorithm fills off-RXS recipient pixels by computing sums of squared differences (a cost function F) between their spectral radiances and those of potential donor pixels/columns on the RXS. Of the RXS pixels with F lower than a certain value, the one with the smallest Euclidean distance to the recipient pixel is designated as the donor, and its retrieved cloud properties and other attributes such as 1D radiative heating rates are consigned to the recipient. It is shown that both the RXS itself and Moderate Resolution Imaging Spectroradiometer (MODIS) imagery can be reconstructed extremely well using just visible and thermal infrared channels. Suitable donors usually lie within 10 km of the recipient. RXSs and their associated radiative heating profiles are reconstructed best for extensive planar clouds and less reliably for broken convective clouds.
Domain-average 1D broadband radiative fluxes at the top of the atmosphere (TOA) for (21 km) 2 domains constructed from MODIS, CloudSat and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) data agree well with coincidental values derived from Clouds and the Earth's Radiant Energy System (CERES) radiances: differences between modelled and measured reflected shortwave fluxes are within +/- 10 Wm(-2) for similar to 35% of the several hundred domains constructed for eight orbits. Correspondingly, for outgoing longwave radiation similar to 65% are within +/- 10 W m(-2). Copyright (C) 2011 Royal Meteorological Society and Crown in the right of Canada.
C1 [Barker, H. W.] Environm Canada, Cloud Phys & Severe Weather Res Sect ARMP, Toronto, ON M3H 5T4, Canada.
[Wehr, T.] European Space Agcy, NL-2200 AG Noordwijk, Netherlands.
[Kato, S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Donovan, D. P.] KNMI, De Bilt, Netherlands.
[Hogan, R. J.] Univ Reading, Reading, Berks, England.
RP Barker, HW (reprint author), Environm Canada, Cloud Phys & Severe Weather Res Sect ARMP, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada.
EM howard.barker@ec.gc.ca
RI Hogan, Robin/M-6549-2016
OI Hogan, Robin/0000-0002-3180-5157
FU European Space Agency
FX This study was supported by a contract issued to Environment Canada by
the European Space Agency under the EarthCARE component of its Living
Planet Programme.
NR 36
TC 24
Z9 24
U1 0
U2 12
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2011
VL 137
IS 657
BP 1042
EP 1058
DI 10.1002/qj.824
PN B
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 777CU
UT WOS:000291592800016
ER
PT J
AU Liu, Z
Ostrenga, D
Leptoukh, G
AF Liu, Zhong
Ostrenga, Dana
Leptoukh, Gregory
TI ONLINE VISUALIZATION AND ANALYSIS OF GLOBAL HALF-HOURLY INFRARED
SATELLITE DATA
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [Liu, Zhong] George Mason Univ, CSISS, Fairfax, VA 22030 USA.
[Liu, Zhong; Ostrenga, Dana; Leptoukh, Gregory] NASA, Goddard Space Flight Ctr, NASA Goddard Earth Sci GES, Data & Informat Serv Ctr DISC, Greenbelt, MD 20771 USA.
[Ostrenga, Dana] ADNET Syst, Rockville, MD USA.
RP Liu, Z (reprint author), George Mason Univ, CSISS, 4400 Univ Dr,MSN 6E1, Fairfax, VA 22030 USA.
EM Zhong.Liu@nasa.gov
NR 3
TC 1
Z9 1
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 APR
PY 2011
VL 92
IS 4
BP 429
EP 432
DI 10.1175/2010BAMS2976.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 773QT
UT WOS:000291323900002
ER
PT J
AU Gorchakov, GI
Sviridenkov, MA
Semoutnikova, EG
Chubarova, NY
Holben, BN
Smirnov, AV
Emilenko, AS
Isakov, AA
Kopeikin, VM
Karpov, AV
Lezina, EA
Zadorozhnaya, OS
AF Gorchakov, G. I.
Sviridenkov, M. A.
Semoutnikova, E. G.
Chubarova, N. Y.
Holben, B. N.
Smirnov, A. V.
Emilenko, A. S.
Isakov, A. A.
Kopeikin, V. M.
Karpov, A. V.
Lezina, E. A.
Zadorozhnaya, O. S.
TI Optical and microphysical parameters of the aerosol in the smoky
atmosphere of the Moscow region in 2010
SO DOKLADY EARTH SCIENCES
LA English
DT Article
ID SURFACE AEROSOL; FIRES
C1 [Gorchakov, G. I.; Sviridenkov, M. A.; Emilenko, A. S.; Isakov, A. A.; Kopeikin, V. M.; Karpov, A. V.] Russian Acad Sci, Oboukhov Inst Atmospher Phys, Moscow 109017, Russia.
[Semoutnikova, E. G.; Lezina, E. A.; Zadorozhnaya, O. S.] Mosekomonitoring, Moscow 119019, Russia.
[Chubarova, N. Y.] Moscow MV Lomonosov State Univ, Moscow 119899, Russia.
[Holben, B. N.; Smirnov, A. V.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Gorchakov, GI (reprint author), Russian Acad Sci, Oboukhov Inst Atmospher Phys, Pyzhevskii Per 3, Moscow 109017, Russia.
EM gengor@ifaran.ru
RI Smirnov, Alexander/C-2121-2009
OI Smirnov, Alexander/0000-0002-8208-1304
FU Russian Foundation for Basic Research [10-05-01019]
FX This work was supported in part by the Russian Foundation for Basic
Research (project no. 10-05-01019).
NR 14
TC 17
Z9 17
U1 0
U2 3
PU MAIK NAUKA/INTERPERIODICA/SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA
SN 1028-334X
J9 DOKL EARTH SCI
JI Dokl. Earth Sci.
PD APR
PY 2011
VL 437
IS 2
BP 513
EP 517
DI 10.1134/S1028334X11040131
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 763PH
UT WOS:000290571700016
ER
PT J
AU Bhagwat, MJ
AF Bhagwat, Mahendra J.
TI Effect of Blade Number on Induced Power in Hover
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
AB Hover performance is thought to be primarily affected by rotor solidity, and it has been suggested that the blade number does not have any effect on performance while comparing rotors with the same solidity. Vortex theory inherently includes the blade number effect but does not account for chord or solidity. For example, Goldstein's classical theory for lightly loaded propellers shows the effect of blade number (independent from blade chord or solidity) on optimum loading and induced power. Simpler analytical formulations, while less accurate, are more useful for understanding these effects. This paper employs combined blade element momentum theory augmented with a finite blade number or "tip loss" effect, using Prandtl's approximation to Goldstein's theory to study induced power in hover. An examination of induced flow effects resulting from finite blade number suggests, contrary to conventional wisdom, that blade number, and not just solidity, has a primary influence on the induced power in hover. Blade aspect ratio or mean nondimensional chord, the other constituent in solidity, appears to have a much smaller and secondary influence. This paper further addresses similarity considerations that can be applied to understand induced power trends.
C1 USA, Res Dev & Engn Command, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Moffett Field, CA USA.
RP Bhagwat, MJ (reprint author), USA, Res Dev & Engn Command, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Moffett Field, CA USA.
EM mahendra.bhagwat@us.army.mil
NR 14
TC 1
Z9 1
U1 0
U2 1
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2011
VL 56
IS 2
AR 022002
DI 10.4050/JAHS.56.022002
PG 8
WC Engineering, Aerospace
SC Engineering
GA 761RF
UT WOS:000290415000002
ER
PT J
AU Datta, A
Johnson, W
AF Datta, Anubhav
Johnson, Wayne
TI Three-Dimensional Finite Element Formulation and Scalable Domain
Decomposition for High-Fidelity Rotor Dynamic Analysis
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID ELLIPTIC PROBLEMS; SUBSTRUCTURING METHODS; PRECONDITIONERS;
CONSTRUCTION; CONSTRAINTS; FETI
AB This paper implements and analyzes a dual-primal iterative substructuring method that is parallel and scalable for the solution of a three-dimensional finite element based dynamic analysis of helicopter rotor blades. The analysis is developed using isoparametric hexahedral brick finite elements. Particular emphasis is placed on the formulation of the inertial terms that are unique to rotary wing dynamics. The scalability of the solution method is studied using two prototype problems one for steady hover (symmetric) and one for transient forward flight (nonsymmetric)-both carried out on up to 48 processors with each substructure on a separate processor. In both hover and forward flight, a linear speedup is observed with number of processors, up to the point of substructure optimality. Substructure optimality and the linear speedup range are shown to depend both on the problem size as well as a corner-based global coarse problem selection. An increase in problem size extends the linear speedup range up to a new substructure optimality. A smaller coarse problem selection extends optimality to a greater number of processors. The key conclusion is that a three-dimensional finite element analysis of a helicopter rotor can be carried out in a fully parallel and scalable manner. The careful selection of substructure corner nodes that are used to construct the global coarse problem is key to extending linear speedup to as high a processor number as possible, thus minimizing the solution time for a given problem size.
C1 [Datta, Anubhav] NASA, Ames Res Ctr, Sci & Technol Corp, USA,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA.
[Johnson, Wayne] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA.
RP Datta, A (reprint author), NASA, Ames Res Ctr, Sci & Technol Corp, USA,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA.
EM datta@merlin.arc.nasa.gov
FU U.S. Department of Defense HPC Modernization Program Office
FX Material presented in this paper is a product of the CREATE-AV Element
of the Computational Research and Engineering for Acquisition Tools and
Environments (CREATE) Program sponsored by the U.S. Department of
Defense HPC Modernization Program Office. This research is conducted at
the U. S. Army Aeroflightdynamics Directorate as part of the HPC
Institute of Advanced Rotorcraft Modeling and Simulation (HI-ARMS) led
by Dr. Roger Strawn.
NR 35
TC 0
Z9 0
U1 0
U2 3
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2011
VL 56
IS 2
AR 022003
DI 10.4050/JAHS.56.022003
PG 14
WC Engineering, Aerospace
SC Engineering
GA 761RF
UT WOS:000290415000003
ER
PT J
AU Taroyan, Y
Erdelyi, R
Bradshaw, SJ
AF Taroyan, Y.
Erdelyi, R.
Bradshaw, S. J.
TI Observational Signatures of Impulsively Heated Coronal Loops: Power-Law
Distribution of Energies
SO SOLAR PHYSICS
LA English
DT Article
DE Heating, coronal; Flares, microflares and nanoflares; Spectral line,
intensity and diagnostics
ID SOLAR; NANOFLARES; OSCILLATIONS; STATISTICS; HINODE; FLARES; WAVES
AB It has been established that small scale heating events, known as nanoflares, are important for solar coronal heating if the power-law distribution of their energies has a slope alpha steeper than -2 (alpha < -2). Forward modeling of impulsively heated coronal loops with a set of prescribed power-law indices alpha is performed. The power-law distribution is incorporated into the governing equations of motion through an impulsive heating term. The results are converted into synthetic Hinode/EIS observations in the 40 '' imaging mode, using a selection of spectral lines formed at various temperatures. It is shown that the intensities of the emission lines and their standard deviations are sensitive to changes in alpha. A method based on a combination of observations and forward modeling is proposed for determining whether the heating in a particular case is due to small or large scale events. The method is extended and applied to a loop structure that consists of multiple strands.
C1 [Taroyan, Y.] Aberystwyth Univ, Inst Math & Phys, Aberystwyth, Dyfed, Wales.
[Erdelyi, R.] Univ Sheffield, Dept Appl Math, SP2RC, Sheffield, S Yorkshire, England.
[Bradshaw, S. J.] Rice Univ, Dept Phys & Astron, Houston, TX USA.
[Bradshaw, S. J.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Taroyan, Y (reprint author), Aberystwyth Univ, Inst Math & Phys, Aberystwyth, Dyfed, Wales.
EM yot@aber.ac.uk; Robertus@sheffield.ac.uk; stephen.bradshaw@nasa.gov
FU NSF, Hungary [K67746]
FX R.E. acknowledges NSF, Hungary (OTKA, ref. no. K67746) and M. Keray for
patient encouragement.
NR 30
TC 5
Z9 5
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD APR
PY 2011
VL 269
IS 2
BP 295
EP 307
DI 10.1007/s11207-010-9702-5
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 762DE
UT WOS:000290451700005
ER
PT J
AU Xu, YS
Fu, LL
AF Xu, Yongsheng
Fu, Lee-Lueng
TI Global Variability of the Wavenumber Spectrum of Oceanic Mesoscale
Turbulence
SO JOURNAL OF PHYSICAL OCEANOGRAPHY
LA English
DT Article
ID GEOSTROPHIC TURBULENCE; ENERGY; ALTIMETER; FLOW; TOPEX/POSEIDON;
SIMULATIONS; INSTABILITY; EDDIES; SCALES
AB The wavenumber spectra of sea surface height from satellite altimeter observations have revealed complex spatial variability that cannot be explained by a universal theory of mesoscale turbulence. Near the edge of the core regions of high eddy energy, agreement is observed with the prediction of the surface quasigeostrophic (SQG) turbulence theory, which has fundamental differences from that of the traditional quasigeostrophic (QG) turbulence theory. In the core regions of high eddy energy, the spectra are consistent with frontogenesis that is not fully accounted for by the SQG theory. However, the observations in the vast ocean interior of low eddy energy exhibit substantial differences from the predictions of existing theories of oceanic mesoscale turbulence. The spectra in these regions may reflect the ocean's response to short-scale atmospheric forcing and air sea interaction. The observations presented in this paper serve as a test bed for new theories and ocean general circulation models.
C1 [Xu, Yongsheng; Fu, Lee-Lueng] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Xu, YS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM yongsheng.xu@jpl.nasa.gov
FU National Aeronautics and Space Administration; Jason-1; OSTM/Jason-2
FX The research presented in the paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. Support
from the Jason-1 and OSTM/Jason-2 projects is acknowledged. The authors
thank Raffaele Ferrari, James McWilliams, Dudley Chelton, and Patrice
Klein for their comments.
NR 25
TC 34
Z9 34
U1 0
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-3670
J9 J PHYS OCEANOGR
JI J. Phys. Oceanogr.
PD APR
PY 2011
VL 41
IS 4
BP 802
EP 809
DI 10.1175/2010JPO4558.1
PG 8
WC Oceanography
SC Oceanography
GA 757AV
UT WOS:000290057200009
ER
PT J
AU Hesse, M
Birn, J
Zenitani, S
AF Hesse, Michael
Birn, Joachim
Zenitani, Seiji
TI Magnetic reconnection in a compressible MHD plasma
SO PHYSICS OF PLASMAS
LA English
DT Article
ID PARALLEL ELECTRIC-FIELDS
AB Using steady-state resistive MHD, magnetic reconnection is reinvestigated for conditions of high resistivity/low magnetic Reynolds number, when the thickness of the diffusion region is no longer small compared to its length. Implicit expressions for the reconnection rate and other reconnection parameters are derived based on the requirements of mass, momentum, and energy conservation. These expressions are solved via simple iterative procedures. Implications specifically for low Reynolds number/high resistivity are being discussed. (C) 2011 American Institute of Physics. [doi:10.1063/1.3581077]
C1 [Hesse, Michael; Zenitani, Seiji] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Birn, Joachim] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Hesse, M (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
RI Hesse, Michael/D-2031-2012; Zenitani, Seiji/D-7988-2013; NASA MMS,
Science Team/J-5393-2013
OI Zenitani, Seiji/0000-0002-0945-1815; NASA MMS, Science
Team/0000-0002-9504-5214
FU NASA's MMS mission; ROSES program; JSPS
FX The authors gratefully acknowledge the support by NASA's MMS mission and
ROSES program. One of us (S.Z.) gratefully acknowledges the support from
JSPS Fellowship for Research Abroad.
NR 24
TC 7
Z9 7
U1 0
U2 2
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 APR
PY 2011
VL 18
IS 4
AR 042104
DI 10.1063/1.3581077
PG 10
WC Physics, Fluids & Plasmas
SC Physics
GA 757TI
UT WOS:000290110200006
ER
PT J
AU Jacquot, BC
Monacos, SP
Hoenk, ME
Greer, F
Jones, TJ
Nikzad, S
AF Jacquot, Blake C.
Monacos, Steve P.
Hoenk, Michael E.
Greer, Frank
Jones, Todd J.
Nikzad, Shouleh
TI A system and methodologies for absolute quantum efficiency measurements
from the vacuum ultraviolet through the near infrared
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID CHARGE-COUPLED-DEVICE; DELTA-DOPED CCDS; SILICON PHOTODIODES; UV;
DETECTORS; PRESSURE; GROWTH; NM
AB In this paper we present our system design and methodology for making absolute quantum efficiency (QE) measurements through the vacuum ultraviolet (VUV) and verify the system with delta-doped silicon CCDs. Delta-doped detectors provide an excellent platform to validate measurements through the VUV due to their enhanced UV response. The requirements for measuring QE through the VUV are more strenuous than measurements in the near UV and necessitate, among other things, the use of a vacuum monochromator, good dewar chamber vacuum to prevent on-chip condensation, and more stringent handling requirements. (C) 2011 American Institute of Physics. [doi:10.1063/1.3574220]
C1 [Jacquot, Blake C.; Monacos, Steve P.; Hoenk, Michael E.; Greer, Frank; Jones, Todd J.; Nikzad, Shouleh] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jacquot, BC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bcj7@cornell.edu; snikzad@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We gratefully acknowledge Patrick Morrissey for discussions on quantum
yield and Tom Elliott for support of Cassini devices. We thank Dr.
Geoffrey James for information and great discussions related to the
measurement system as well as generous equipment contributions. We also
thank the reviewer of this manuscript for extensive and thoughtful
comments that improved the quality of this paper. The research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 21
TC 9
Z9 9
U1 0
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD APR
PY 2011
VL 82
IS 4
AR 043102
DI 10.1063/1.3574220
PG 10
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 756YU
UT WOS:000290051500002
PM 21528990
ER
PT J
AU Wang, RH
Burleigh, SC
Parikh, P
Lin, CJ
Sun, B
AF Wang, Ruhai
Burleigh, Scott C.
Parikh, Paavan
Lin, Che-Jen (Jerry)
Sun, Bo
TI Licklider Transmission Protocol (LTP)-Based DTN for Cislunar
Communications
SO IEEE-ACM TRANSACTIONS ON NETWORKING
LA English
DT Article
DE Bundle Protocol (BP); delay-tolerant networking (DTN); interplanetary
Internet (IPN); Licklider Transmission Protocol convergence layer
(LTPCL); satellite communications; Transmission Control Protocol
convergence layer (TCPCL)
ID INTERPLANETARY INTERNET; TRANSPORT PROTOCOL; SATELLITE NETWORKS;
CONGESTION CONTROL; SPACE-INTERNET; PERFORMANCE; ARCHITECTURE; TCP/IP;
LINKS
AB Delay/disruption-tolerant networking (DTN) technology offers a new solution to highly stressed communications in space environments, especially those with long link delay and frequent link disruptions in deep-space missions. To date, little work has been done in evaluating the performance of the available "convergence layer" protocols of DTN, especially the Licklider Transmission Protocol (LTP), when they are applied to an interplanetary Internet (IPN). In this paper, we present an experimental evaluation of the Bundle Protocol (BP) running over various "convergence layer" protocols in a simulated cislunar communications environment characterized by varying degrees of signal propagation delay and data loss. We focus on the LTP convergence layer (LTPCL) adapter running on top of UDP/IP (i.e., BP/LTPCL/UDP/IP). The performance of BP/LTPCL/UDP/IP in realistic file transfers over a PC-based network test bed is compared to that of two other DTN protocol stack options, BP/TCPCL/TCP/IP and BP/UDPCL/UDP/IP. A statistical method of t-test is also used for analysis of the experimental results. The experiment results show that LTPCL has a significant performance advantage over Transmission Control Protocol convergence layer (TCPCL) for link delays longer than 4000 ms regardless of the bit error rate (BER). For a very lossy channel with a BER of around 10(-5), LTPCL has a significant goodput advantage over TCPCL at all the link delay levels studied, with an advantage of around 3000 B/s for delays longer than 1500 ms. LTPCL has a consistently significant goodput advantage over UDPCL, around 2500-3000 B/s, at all levels of link delays and BERs.
C1 [Wang, Ruhai] Soochow Univ, Sch Elect & Informat Engn, Suzhou 215006, Peoples R China.
[Wang, Ruhai; Parikh, Paavan] Lamar Univ, Phillip M Drayer Dept Elect Engn, Beaumont, TX 77710 USA.
[Burleigh, Scott C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lin, Che-Jen (Jerry)] Lamar Univ, Dept Civil Engn, Beaumont, TX 77710 USA.
[Sun, Bo] Lamar Univ, Dept Comp Sci, Beaumont, TX 77710 USA.
RP Wang, RH (reprint author), Soochow Univ, Sch Elect & Informat Engn, Suzhou 215006, Peoples R China.
EM rwang@lamar.edu; scott.c.burleigh@jpl.nasa.gov; pparikh@lamar.edu;
jerry.lin@lamar.edu; bo.sun@lamar.edu
RI yu, yan/C-2322-2012; Lin, Che-Jen/K-1808-2013
OI Lin, Che-Jen/0000-0001-5990-3093
FU National Aeronautics and Space Administration; National Natural Science
Foundation of China (NSFC) [61032003]
FX Manuscript received March 03, 2009; revised March 02, 2010 and July 06,
2010; accepted July 17, 2010; approved by IEEE/ACM TRANSACTIONS ON
NETWORKING Editor M. Liu. Date of publication December 17, 2010; date of
current version April 15, 2011. The research described in this paper was
performed in part at the Jet Propulsion Laboratory, California Institute
of Technology, Pasadena, under a contract with the National Aeronautics
and Space Administration, supported in part by the National Natural
Science Foundation of China (NSFC) under Grant 61032003.
NR 51
TC 32
Z9 34
U1 2
U2 14
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1063-6692
J9 IEEE ACM T NETWORK
JI IEEE-ACM Trans. Netw.
PD APR
PY 2011
VL 19
IS 2
BP 359
EP 368
DI 10.1109/TNET.2010.2060733
PG 10
WC Computer Science, Hardware & Architecture; Computer Science, Theory &
Methods; Engineering, Electrical & Electronic; Telecommunications
SC Computer Science; Engineering; Telecommunications
GA 754HM
UT WOS:000289845700005
ER
PT J
AU Moayeri, N
Mapar, J
Tompkins, S
Pahlavan, K
AF Moayeri, Nader
Mapar, Jalal
Tompkins, Stefanie
Pahlavan, Kaveh
TI EMERGING OPPORTUNITIES FOR LOCALIZATION AND TRACKING
SO IEEE WIRELESS COMMUNICATIONS
LA English
DT Editorial Material
C1 [Moayeri, Nader] NIST, Gaithersburg, MD 20899 USA.
[Moayeri, Nader] Hewlett Packard Labs, Imaging Technol Dept, Palo Alto, CA USA.
[Moayeri, Nader] Rutgers State Univ, Dept Elect & Comp Engn, Piscataway, NJ 08855 USA.
[Mapar, Jalal] SAIC, RDT&E, Mclean, VA USA.
[Tompkins, Stefanie] NASA, Washington, DC 20546 USA.
[Pahlavan, Kaveh] Worcester Polytech Inst, Ctr Wireless Informat Network Studies, Worcester, MA USA.
RP Moayeri, N (reprint author), NIST, Gaithersburg, MD 20899 USA.
EM nader.moayeri@nist.gov; Jalal.Mapar@dhs.gov;
Stefanie.Tompkins@darpa.mil; kavehpahlavan@gmail.com
NR 0
TC 9
Z9 9
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1536-1284
J9 IEEE WIREL COMMUN
JI IEEE Wirel. Commun.
PD APR
PY 2011
VL 18
IS 2
BP 8
EP 9
PG 2
WC Computer Science, Hardware & Architecture; Computer Science, Information
Systems; Engineering, Electrical & Electronic; Telecommunications
SC Computer Science; Engineering; Telecommunications
GA 753PI
UT WOS:000289791500004
ER
PT J
AU Fridlind, AM
Ackerman, AS
AF Fridlind, Ann M.
Ackerman, Andrew S.
TI Estimating the Sensitivity of Radiative Impacts of Shallow, Broken
Marine Clouds to Boundary Layer Aerosol Size Distribution Parameter
Uncertainties for Evaluation of Satellite Retrieval Requirements
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID TRADE-WIND CUMULI; CLIMATE; CONVECTION; SIMULATIONS; CONSEQUENCES;
MODELS; ALBEDO
AB A proposed objective of the planned Aerosol-Cloud-Ecosystem (ACE) satellite mission is to provide constraints on climate model representation of aerosol effects on clouds by retrieving profiles of aerosol number concentration, effective variance, and effective radius over the 0.1-1-mu m radius range under humidified ambient conditions with 500-m vertical resolution and uncertainties of 100%, 50%. and 10%, respectively. Shallow, broken marine clouds provide an example of conditions where boundary layer aerosol properties would be retrieved in clear-sky gaps. To quantify the degree of constraint that proposed retrievals might provide on cloud radiative forcing (CRF) simulated by climate models under such conditions, dry aerosol size distribution parameters are independently varied here in large-eddy simulations of three well-established modeling case studies. Using the rudimentary available aerosol specifications, it is found that relative changes of total dry aerosol properties in simulations can be used as a proxy for relative changes of ambient aerosol properties targeted by ACE retrievals. The sensitivity of simulated daytime shortwave CRF to the proposed uncertainty in retrieved aerosol number concentration is -15 W m(-2) in the overcast limit, roughly a factor of 2 smaller than a simple analytic estimate owing primarily to aerosol-induced reductions in simulated liquid water path across this particular set of case studies. The CRF sensitivity to proposed uncertainties in retrieved aerosol effective variance and effective radius is typically far smaller, with no corresponding analytic estimate. Generalization of the results obtained here using only three case studies would require statistical analysis of relevant meteorological and aerosol observations and quantification of observational and model uncertainties and biases.
C1 [Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Fridlind, AM (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM ann.fridlind@nasa.gov
RI Ackerman, Andrew/D-4433-2012; Fridlind, Ann/E-1495-2012
OI Ackerman, Andrew/0000-0003-0254-6253;
FU NASA; NASA Advanced Supercomputing Division
FX Financial and computational support was provided by the NASA Radiation
Sciences Program and the NASA Advanced Supercomputing Division. We thank
three anonymous reviewers and the authors of NASA's ACE white papers for
useful comments. We thank Alexander Avramov for contributions to model
analysis.
NR 30
TC 4
Z9 4
U1 0
U2 2
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 APR
PY 2011
VL 28
IS 4
BP 530
EP 538
DI 10.1175/2010JTECHA1520.1
PG 9
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 757AZ
UT WOS:000290057600006
ER
PT J
AU Wagner, D
Papastamatiou, YP
Kosaki, RK
Gleason, KA
McFall, GB
Boland, RC
Pyle, RL
Toonen, RJ
AF Wagner, Daniel
Papastamatiou, Yannis P.
Kosaki, Randall K.
Gleason, Kelly A.
McFall, Greg B.
Boland, Raymond C.
Pyle, Richard L.
Toonen, Robert J.
TI New Records of Commercially Valuable Black Corals (Cnidaria:
Antipatharia) from the Northwestern Hawaiian Islands at Mesophotic
Depths
SO PACIFIC SCIENCE
LA English
DT Article
ID ANTHOZOA ANTIPATHARIA; CARIJOA-RIISEI; ZOOGEOGRAPHY; SYSTEMATICS;
ACROPORA
AB Mesophotic coral reef ecosystems are notoriously undersurveyed worldwide and particularly in remote locations like the Northwestern Hawaiian Islands (NWHI). A total of 37 mixed-gas technical dives were performed to depths of 80 m across the NWHI to survey for the presence of the invasive octocoral Carijoa sp., the invasive red alga Acanthophora spicifera, and conspicuous megabenthic fauna such as black corals. The two invasive species were not recorded from any of the surveys, but two commercially valuable black coral species, Antipathes griggi and Myriopathes ulex, were found, representing substantial range expansions for these species. Antipathes griggi was recorded from the islands of Necker and Laysan in 58-70 m, and Myriopathes ulex was recorded from Necker Island and Pearl and Hermes Atoll in 58-70 in. Despite over 30 yr of research in the NWHI, these black coral species had remained undetected. The new records of these conspicuous marine species highlight the utility of deep-diving technologies in surveying the largest part of the depth range of coral reef ecosystems (40-150 m), which remains largely unexplored.
C1 [Wagner, Daniel; Toonen, Robert J.] Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA.
[Papastamatiou, Yannis P.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Kosaki, Randall K.; Gleason, Kelly A.] NOAA Papahanaumokuakea Marine Natl Monument, Honolulu, HI 96825 USA.
[McFall, Greg B.] NOAA, Natl Marine Sanctuary Program, Savannah, GA 31411 USA.
[Boland, Raymond C.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
[Pyle, Richard L.] Bernice P Bishop Museum, Honolulu, HI 96817 USA.
RP Wagner, D (reprint author), Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA.
EM wagnerda@hawaii.edu
RI Toonen, Rob/K-2891-2012
OI Toonen, Rob/0000-0001-6339-4340
FU Western Pacific Fisheries Management Council to the University of
Hawai'i through the NOAA [NA07N-MF4410114]; NSF [OCE-0623678]; NMSP MOA
[2005-008/66882]
FX This work was funded in part by the Western Pacific Fisheries Management
Council to the University of Hawai'i through the NOAA Coral Reef
Conservation Giant Program under award number NA07N-MF4410114, NSF
OCE-0623678, and NMSP MOA#2005-008/66882. This is HIMR contribution 1395
and SOEST 7986. Manuscript accepted 30 July 2010.
NR 43
TC 8
Z9 10
U1 0
U2 6
PU UNIV HAWAII PRESS
PI HONOLULU
PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA
SN 0030-8870
J9 PAC SCI
JI Pac. Sci.
PD APR
PY 2011
VL 65
IS 2
BP 249
EP 255
DI 10.2984/65.2.249
PG 7
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 753WV
UT WOS:000289811900008
ER
PT J
AU Grav, T
Jedicke, R
Denneau, L
Chesley, S
Holman, MJ
Spahr, TB
AF Grav, Tommy
Jedicke, Robert
Denneau, Larry
Chesley, Steve
Holman, Matthew J.
Spahr, Timothy B.
TI The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and
Efficiency Determination of the Moving Object Processing System
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID JOVIAN TROJAN ASTEROIDS; JUPITER-FAMILY COMETS; LONG-PERIOD COMETS;
NEAR-EARTH OBJECTS; KUIPER-BELT; SIZE DISTRIBUTION; MAGNITUDE
DISTRIBUTION; POPULATION; CENTAURS; ORIGIN
AB We present here the Pan-STARRS Moving Object Processing System (MOPS) Synthetic Solar System Model (S3M), the first-ever attempt at building a comprehensive flux-limited model of the major small-body populations in the solar system. The goal of the S3M is to provide a valuable tool in the design and testing of the MOPS software, and will be used in the monitoring of the upcoming Pan-STARRS 1 all-sky survey, which started science operations during late spring of 2010. The model is composed of synthetic populations of near-Earth objects (NEOs with a subpopulation of Earth impactors), the main-belt asteroids (MBAs), Jovian Trojans, Centaurs, trans-Neptunian objects (classical, resonant, and scattered trans-Neptunian objects [TNOs]), Jupiter-family comets (JECs), long-period comets (LPCs), and interstellar comets. The model reasonably reproduces the true populations to a minimum of V = 24.5, corresponding to approximately the expected limiting magnitude for Pan-STARRS's ability to detect moving objects. The NEO synthetic population has been extended to H < 25 (corresponding to objects of about 50 m in diameter), allowing for close flybys of the Earth to be modeled.
C1 [Grav, Tommy] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Jedicke, Robert; Denneau, Larry] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Chesley, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Holman, Matthew J.; Spahr, Timothy B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
RP Grav, T (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM tgrav@pha.jhu.edu; jedicke@ifa.hawaii.edu; denneau@ifa.hawaii.edu;
steve.chesley@jpl.nasa.gov; mholman@cfa.harvard.edu;
tspahr@cfa.harvard.cdu
FU US Air Force Research Laboratory (Albuquerque, New Mexico)
[F29601-02-1-0268]
FX The design and construction of the Panoramic Survey Telescope and Rapid
Response System by the University of Hawaii Institute for Astronomy is
funded by the US Air Force Research Laboratory (Albuquerque, New Mexico)
through grant number F29601-02-1-0268. This work was conducted in part
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 70
TC 24
Z9 24
U1 0
U2 1
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 APR
PY 2011
VL 123
IS 902
BP 423
EP 447
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 757YM
UT WOS:000290124900005
ER
PT J
AU Vilozny, B
Actis, P
Seger, RA
Pourmand, N
AF Vilozny, Boaz
Actis, Paolo
Seger, R. Adam
Pourmand, Nader
TI Dynamic Control of Nanoprecipitation in a Nanopipette
SO ACS NANO
LA English
DT Article
DE nanoprecipitation; nanopipette; nanopore; ion current rectification;
current oscillations
ID POTENTIAL BIOMEDICAL APPLICATIONS; CONICAL NANOPORE SENSOR; CURRENT
RECTIFICATION; NANOPARTICLES; OSCILLATIONS; ZINC
AB Studying the earliest, stages of precipitation at the nanoscale is technically challenging but quite valuable as such phenomena reflect important processes such as crystallization and biomineralization. Using a quartz nanopipette as a nanoreactor, we induced precipitation of an insoluble salt to generate oscillating current blockades. The reversible process can be used to measure both kinetics of precipitation and relative size of the resulting nanoparticles. Counter ions for the highly water-Insoluble salt zinc phosphate were separated by the pore of a nanopipette and a potential applied to cause ion migration to the Interface. By analyzing the kinetics of pore blockage, two distinct mechanisms were identified: a slower process due to precipitation from solution, and a faster process attributed to voltage-driven migration of a trapped precipitate. We discuss the potential of these techniques in studying precipitation dynamics, trapping particles within a nanoreactor, and electrical sensors based on nanoprecipitation.
C1 [Vilozny, Boaz; Actis, Paolo; Seger, R. Adam; Pourmand, Nader] Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA.
[Vilozny, Boaz; Actis, Paolo; Seger, R. Adam; Pourmand, Nader] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Vilozny, Boaz; Actis, Paolo; Seger, R. Adam; Pourmand, Nader] UC Santa Cruz, Adv Studies Labs, Moffett Field, CA 94035 USA.
[Actis, Paolo] Texas So Univ, Dept Biol, Houston, TX 77004 USA.
RP Pourmand, N (reprint author), Univ Calif Santa Cruz, Dept Biomol Engn, 1156 High St, Santa Cruz, CA 95064 USA.
EM pourmand@soe.ucsc.edu
RI babakinejad, babak/G-2674-2012; Actis, Paolo/A-7694-2012
FU National Aeronautics and Space Administration [NNX10AQ16A, NNX08BA47A];
National Institutes of Health [P01-HG000205]
FX This work was supported in part by grants from the National Aeronautics
and Space Administration Cooperative Agreements NNX10AQ16A and
NNX08BA47A, and the National Institutes of Health [P01-HG000205].
NR 32
TC 12
Z9 12
U1 8
U2 55
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1936-0851
J9 ACS NANO
JI ACS Nano
PD APR
PY 2011
VL 5
IS 4
BP 3191
EP 3197
DI 10.1021/nn200320b
PG 7
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 753CJ
UT WOS:000289742100090
PM 21413733
ER
PT J
AU Schubert, WW
Beaudet, RA
AF Schubert, Wayne W.
Beaudet, Robert A.
TI Determination of Lethality Rate Constants and D-Values for
Heat-Resistant Bacillus Spores ATCC 29669 Exposed to Dry Heat from 125
degrees C to 200 degrees C
SO ASTROBIOLOGY
LA English
DT Article
DE Bacillus; Spores; Planetary protection; Dry heat microbial reduction;
ATCC 29669; D-value
ID AIRBORNE BACTERIAL-SPORES; SUBTILIS VAR NIGER; THERMAL-RESISTANCE;
SPACECRAFT; DEATH; MICROORGANISMS; INACTIVATION; KINETICS; CURVES;
SYSTEM
AB Exposing flight hardware to dry heat is a NASA-approved sterilization method for reducing microbial bioburden on spacecraft. The existing NASA specification only allows heating the flight hardware between 104 degrees C and 125 degrees C to reduce the number of viable microbes and bacterial spores. Also, the NASA specifications only allow a four log reduction by dry heat microbial reduction because very heat-resistant spores are presumed to exist in a diverse population (0.1%). The goal of this research was to obtain data at higher temperatures than 125 degrees C for one of the most heat-resistant microorganisms discovered in a spacecraft assembly area. These data support expanding the NASA specifications to temperatures higher than 125 degrees C and relaxing the four log reduction specification.
Small stainless steel vessels with spores of the Bacillus strain ATCC 29669 were exposed to constant temperatures between 125 degrees C and 200 degrees C under both dry and ambient room humidity for set time durations. After exposures, the thermal spore exposure vessels were cooled and the remaining spores recovered and plated out. Survivor ratios, lethality rate constants, and D-values were determined at each temperature. The D-values for the spores exposed under dry humidity conditions were always found to be shorter than those under ambient humidity. The temperature dependence of the lethality rate constants was obtained by assuming that they obeyed Arrhenius behavior. The results are compared to those of B. atrophaeus ATCC 9372. In all cases, the D-values of ATCC 29669 are between 20 and 50 times longer than those of B. atrophaeus ATCC 9372.
C1 [Schubert, Wayne W.; Beaudet, Robert A.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
RP Schubert, WW (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Wayne.W.Schubert@jpl.nasa.gov
FU National Aeronautics and Space Administration; Jet Propulsion Laboratory
Mars Program Office
FX The research described in this paper was carried out by the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Funding
for this work was provided by the Jet Propulsion Laboratory Mars Program
Office, and we thank the Mars Program Planetary Protection Manager Dr.
Karen Buxbaum for her support of this task. We thank Dr. Michael J.
Kempf for his extensive work on developing the methods used in this
study. We also thank Dr. J. Andy Spry from the Biotechnology and
Planetary Protection Group at JPL, J. Rudy Puleo at Kennedy Space
Center, and Dr. Terry Foster (TVF, Inc., The Woodlands, TX), for their
helpful comments and discussions. A new technology report (JPL,
NTR-47399) was submitted describing the use of these heat-resistant
spores of this bacterial strain.
NR 27
TC 3
Z9 4
U1 0
U2 8
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 APR
PY 2011
VL 11
IS 3
BP 213
EP 223
DI 10.1089/ast.2010.0502
PG 11
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 752GE
UT WOS:000289678500005
PM 21417744
ER
PT J
AU Philip, GK
Freeland, SJ
AF Philip, Gayle K.
Freeland, Stephen J.
TI Did Evolution Select a Nonrandom "Alphabet" of Amino Acids?
SO ASTROBIOLOGY
LA English
DT Article
DE Astrobiology; Evolution; Molecular biology; Modeling studies
ID GENETIC-CODE; GENOMICS
AB The last universal common ancestor of contemporary biology (LUCA) used a precise set of 20 amino acids as a standard alphabet with which to build genetically encoded protein polymers. Considerable evidence indicates that some of these amino acids were present through nonbiological syntheses prior to the origin of life, while the rest evolved as inventions of early metabolism. However, the same evidence indicates that many alternatives were also available, which highlights the question: what factors led biological evolution on our planet to define its standard alphabet? One possibility is that natural selection favored a set of amino acids that exhibits clear, nonrandom properties-a set of especially useful building blocks. However, previous analysis that tested whether the standard alphabet comprises amino acids with unusually high variance in size, charge, and hydrophobicity (properties that govern what protein structures and functions can be constructed) failed to clearly distinguish evolution's choice from a sample of randomly chosen alternatives. Here, we demonstrate unambiguous support for a refined hypothesis: that an optimal set of amino acids would spread evenly across a broad range of values for each fundamental property. Specifically, we show that the standard set of 20 amino acids represents the possible spectra of size, charge, and hydrophobicity more broadly and more evenly than can be explained by chance alone.
C1 [Philip, Gayle K.; Freeland, Stephen J.] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Freeland, SJ (reprint author), Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
EM freeland@ifa.hawaii.edu
OI Philip, Gayle/0000-0002-2671-5093
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNA09DA77A]
FX We acknowledge the access provided to the computational facilities of
the Bioinformatics research unit at NUI Maynooth. This research was
supported by the National Aeronautics and Space Administration through
the NASA Astrobiology Institute under Cooperative Agreement No.
NNA09DA77A issued through the Office of Space Science.
NR 21
TC 13
Z9 13
U1 1
U2 18
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 APR
PY 2011
VL 11
IS 3
BP 235
EP 240
DI 10.1089/ast.2010.0567
PG 6
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 752GE
UT WOS:000289678500007
PM 21434765
ER
PT J
AU Thompson, AM
Oltmans, SJ
Tarasick, DW
von der Gathen, P
Smit, HGJ
Witte, JC
AF Thompson, Anne M.
Oltmans, Samuel J.
Tarasick, David. W.
von der Gathen, Peter
Smit, Herman G. J.
Witte, Jacquelyn C.
TI Strategic ozone sounding networks: Review of design and accomplishments
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Review
DE Ozone; Ozonesondes; TTL; Stratosphere-troposphere exchange; Tropospheric
ozone; Tropics; Ozone depleticn
ID TROPICAL TROPOSPHERIC OZONE; MAPPING SPECTROMETER TOMS; DATA
ASSIMILATION SYSTEM; WAVE INDUCED LAMINAE; IN-SITU MEASUREMENTS; ARCTIC
POLAR VORTEX; STRATOSPHERIC OZONE; LOSS RATES; CHEMICAL DEPLETION;
SEASONAL EVOLUTION
AB Ozone soundings are used to integrate models, satellite, aircraft and ground-based measurements for better interpretation of ozone variability, including atmospheric losses (predominantly in the stratosphere) and pollution (troposphere). A well-designed network of ozonesonde stations gives information with high vertical and horizontal resolution on a number of dynamical and chemical processes, allowing us to answer questions not possible with aircraft campaigns or current satellite technology. Strategic ozonesonde networks are discussed for high, mid- and low latitude studies. The Match sounding network was designed specifically to follow ozone depletion within the polar vortex: the standard sites are at middle to high northern hemisphere latitudes and typically operate from December through mid-March. Three mid-latitude strategic networks (the IONS series) operated over North America in July-August 2004, March-May and August 2006, and April and June-July-2008. These were designed to address questions about tropospheric ozone budgets and sources, including stratosphere-troposphere transport, and to validate satellite instruments and models. A global network focusing on processes in the equatorial zone, SHADOZ (Southern Hemisphere Additional Ozonesondes), has operated since 1998 in partnership with NOAA, NASA and the Meteorological Services of host countries. Examples of important findings from these networks are described. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Oltmans, Samuel J.] NOAA, Global Monitoring Div, Environm Syst Res Lab, Boulder, CO 80305 USA.
[Tarasick, David. W.] Environm Canada, Air Qual Res Div, Downsview, ON M3H 5T4, Canada.
[von der Gathen, Peter] Alfred Wegener Inst Polar & Marine Res, D-14473 Potsdam, Germany.
[Smit, Herman G. J.] FZ Juelich, Inst Chem & Dynam Geosphere Troposphere ICG 2, D-52428 Julich, Germany.
[Witte, Jacquelyn C.] NASA, SSAI, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thompson, AM (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
EM amt16@psu.edu; samuel.j.oltmans@noaa.gov; david.tarasick@ec.gc.ca;
peter.von.der.gathen@awi.de; h.smit@fz-juelich.de;
Jacquelyn.witte@nasa.gov
RI von der Gathen, Peter/B-8515-2009; Smit, Herman/J-2397-2012; Thompson,
Anne /C-3649-2014;
OI von der Gathen, Peter/0000-0001-7409-1556; Smit,
Herman/0000-0002-2268-4189; Thompson, Anne /0000-0002-7829-0920;
Tarasick, David/0000-0001-9869-0692
NR 159
TC 28
Z9 29
U1 4
U2 27
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD APR
PY 2011
VL 45
IS 13
BP 2145
EP 2163
DI 10.1016/j.atmosenv.2010.05.002
PG 19
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 753ZG
UT WOS:000289819200001
ER
PT J
AU Voulgarakis, A
Hadjinicolaou, P
Pyle, JA
AF Voulgarakis, A.
Hadjinicolaou, P.
Pyle, J. A.
TI Increases in global tropospheric ozone following an El Nino event:
examining stratospheric ozone variability as a potential driver
SO ATMOSPHERIC SCIENCE LETTERS
LA English
DT Article
DE El Nino; STE; tropospheric ozone; stratospheric ozone
ID SOUTHERN-OSCILLATION; EXCHANGE; CLOUDS; SIMULATIONS; PHOTOLYSIS;
TRANSPORT; PACIFIC; CLIMATE; BUDGET; MODEL
AB The stratosphere can strongly influence the interannual variability of tropospheric ozone. It has been discussed previously that tropospheric ozone can increase following an El Nino event, due to enhanced stratosphere/troposphere exchange (STE) of ozone. Here, we run a chemical-transport model for 5 years, covering a period including a strong El Nino event (1997-1998), and find that variability of ozone in the stratosphere is an almost negligible driver of modelled post-El Nino increases of ozone STE and tropospheric ozone abundances. Changes in the dynamics, affecting the cross-tropopause air-mass flux, may be far more important in driving these anomalies. Copyright. (C) 2011 Royal Meteorological Society
C1 [Voulgarakis, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Voulgarakis, A.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Voulgarakis, A.; Pyle, J. A.] Univ Cambridge, NCAS Climate, Ctr Atmospher Sci, Dept Chem, Cambridge CB2 1TN, England.
[Hadjinicolaou, P.] Cyprus Inst, Energy Environm & Water Res Ctr, Nicosia, Cyprus.
RP Voulgarakis, A (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM avoulgarakis@giss.nasa.gov
RI Hadjinicolaou, Panos/H-1729-2016
OI Hadjinicolaou, Panos/0000-0003-1170-2182
FU NERC; NCAS (UK); IKY (Greece)
FX The authors thank NERC and NCAS (UK) for funding the research presented
here. A. V. thanks IKY (Greece) for financial support and P. Braesicke
for useful discussions on the experimental set-up. We also thank G. D.
Carver for his help with model development and P. Berrisford for
providing ECMWF data.
NR 30
TC 19
Z9 20
U1 3
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1530-261X
J9 ATMOS SCI LETT
JI Atmos. Sci. Lett.
PD APR-JUN
PY 2011
VL 12
IS 2
BP 228
EP 232
DI 10.1002/asl.318
PG 5
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 751WU
UT WOS:000289649200012
ER
PT J
AU Sherrit, S
Bao, XQ
Jones, CM
Aldrich, JB
Blodget, CJ
Moore, JD
Carson, JW
Goullioud, R
AF Sherrit, Stewart
Bao, Xiaoqi
Jones, Christopher M.
Aldrich, Jack B.
Blodget, Chad J.
Moore, James D.
Carson, John W.
Goullioud, Renaud
TI Piezoelectric Multilayer Actuator Life Test
SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL
LA English
DT Article
AB Potential NASA optical missions such as the Space Interferometer Mission require actuators for precision positioning to accuracies of the order of nanometers. Commercially available multilayer piezoelectric stack actuators are being considered for driving these precision mirror positioning mechanisms. These mechanisms have potential mission operational requirements that exceed 5 years for one mission life. To test the feasibility of using these commercial actuators for these applications and to determine their reliability and the redundancy requirements, a life test study was undertaken. The nominal actuator requirements for the most critical actuators on the Space Interferometry Mission (SIM) in terms of number of cycles was estimated from the Modulation Optics Mechanism (MOM) and Pathlength control Optics Mechanism (POM) and these requirements were used to define the study. At a nominal drive frequency of 250 Hz, one mission life is calculated to be 40 billion cycles. In this study, a set of commercial PZT stacks configured in a potential flight actuator configuration (pre-stressed to 18 MPa and bonded in flexures) were tested for up to 100 billion cycles. Each test flexure allowed for two sets of primary and redundant stacks to be mechanically connected in series. The tests were controlled using an automated software control and data acquisition system that set up the test parameters and monitored the waveform of the stack electrical current and voltage. The samples were driven between 0 and 20 V at 2000 Hz to accelerate the life test and mimic the voltage amplitude that is expected to be applied to the stacks during operation. During the life test, 10 primary stacks were driven and 10 redundant stacks, mechanically in series with the driven stacks, were open-circuited. The stroke determined from a strain gauge, the temperature and humidity in the chamber, and the temperature of each individual stack were recorded. Other properties of the stacks, including the displacement from a capacitance gap sensor and impedance spectra were measured at specific intervals. The average degradation in the stroke over the life test was found to be small (<3%) for the primary stacks and <4% for the redundant stacks. It was noted that about half of the stroke reduction occurred within the first 10 billion cycles. At the end of the life test, it was found that the actuator could recover about half of the lost stroke by applying a dc voltage of 100 V at room temperature. The data up to 100 billion cycles for these tests and the analysis of the experimental results are presented in this paper.
C1 [Sherrit, Stewart; Jones, Christopher M.; Aldrich, Jack B.] CALTECH, Jet Prop Lab, Adv Technol Grp, Pasadena, CA 91125 USA.
[Bao, Xiaoqi] CALTECH, Jet Prop Lab, Adv Actuators Team, Pasadena, CA USA.
RP Sherrit, S (reprint author), CALTECH, Jet Prop Lab, Adv Technol Grp, Pasadena, CA 91125 USA.
EM ssherrit@jpl.nasa.gov
FU National Aeronautics Space Agency (NASA)
FX Research reported in this manuscript was conducted at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under a contract
with National Aeronautics Space Agency (NASA). Reference herein to any
specific commercial product, process, or service by trade name,
trademark, manufacturer, or otherwise, does not constitute or imply its
endorsement by the United States Government or the Jet Propulsion
Laboratory, California Institute of Technology.
NR 12
TC 2
Z9 4
U1 2
U2 21
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0885-3010
J9 IEEE T ULTRASON FERR
JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control
PD APR
PY 2011
VL 58
IS 4
BP 820
EP 828
DI 10.1109/TUFFC.2011.1874
PG 9
WC Acoustics; Engineering, Electrical & Electronic
SC Acoustics; Engineering
GA 754EB
UT WOS:000289834500016
PM 21507759
ER
PT J
AU Liu, KC
Chattopadhyay, A
Bednarcyk, B
Arnold, SM
AF Liu, Kuang C.
Chattopadhyay, Aditi
Bednarcyk, Brett
Arnold, Steven M.
TI Efficient Multiscale Modeling Framework for Triaxially Braided
Composites using Generalized Method of Cells
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Micromechanics; Polymer matrix composites; Multiscale modeling;
Triaxially braided composites; Generalized method of cells; Repeating
unit cell; Homogenization; Localization
ID TEXTILE COMPOSITES; COMPRESSIVE RESPONSE; MECHANICAL-BEHAVIOR; STRENGTH;
FAILURE; PREDICTION; DESIGN
AB In this paper, a framework for a three-scale analysis, beginning at the constituent response and propagating to the braid repeating unit cell (RUC) level, is presented. At each scale in the analysis, the response of the appropriate RUC is represented by homogenized effective properties determined from the generalized method of cells micromechanics theory. Two different macroscale RUC architectures are considered, one for eventual finite-element implementation and the other for material design, and their differences are compared. Model validation is presented through comparison to both experimental data and detailed finite-element simulations. Results show good correlation within range of experimental scatter and the finite-element simulation. Results are also presented for parametric studies varying both the overall fiber volume fraction and braid angle. These studies are compared to predictions from classical lamination theory for reference. Finally, the multiscale analysis framework is used to predict the onset of failure in a transversely loaded triaxially braided composite. The predicted transverse failure initiation stress value shows excellent correlation and provides the bound for which linear elastic constitutive models are acceptable for implementation. DOI: 10.1061/(ASCE)AS.1943-5525.0000009. (C) 2011 American Society of Civil Engineers.
C1 [Liu, Kuang C.; Chattopadhyay, Aditi] Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA.
[Bednarcyk, Brett; Arnold, Steven M.] NASA, Mech & Life Predict Branch, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Liu, KC (reprint author), Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA.
NR 20
TC 19
Z9 20
U1 2
U2 15
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2011
VL 24
IS 2
BP 162
EP 169
DI 10.1061/(ASCE)AS.1943-5525.0000009
PG 8
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 752KU
UT WOS:000289690900005
ER
PT J
AU Li, XT
Binienda, WK
Goldberg, RK
AF Li, Xuetao
Binienda, Wieslaw K.
Goldberg, Robert K.
TI Finite-Element Model for Failure Study of Two-Dimensional Triaxially
Braided Composite
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Two-dimensional triaxially braided composite; Unit cell; Progressive
degradation; Cohesive; Debonding; Straight-sided specimen test
ID FRACTURE-TOUGHNESS; PROGRESSIVE DAMAGE; DELAMINATION; IMPACT
AB A new three-dimensional finite-element model of two-dimensional, triaxially braided composites is presented in this paper. This mesoscale modeling technique is used to examine and predict the deformation and damage observed in tests of straight-sided specimens. A unit cell-based approach is used to consider the braiding architecture and the mechanical properties of the fiber tows, the matrix, and the fiber tow-matrix interface. A 0 degrees/ +/- 60 braiding configuration has been investigated by conducting static finite-element analyses. Failure initiation and progressive degradation has been simulated in the fiber tows by using the Hashin failure criteria and a damage evolution law. The fiber tow-matrix interface was modeled by using a cohesive zone approach to capture any fiber-matrix debonding. By comparing the analytical results with those obtained experimentally, the applicability of the developed model was assessed and the failure process was investigated. DOI: 10.1061/(ASCE)AS.1943-5525.0000029. (C) 2011 American Society of Civil Engineers.
C1 [Li, Xuetao; Binienda, Wieslaw K.] Univ Akron, Akron, OH 44325 USA.
[Goldberg, Robert K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Li, XT (reprint author), Univ Akron, Akron, OH 44325 USA.
EM xl17@zips.uakron.edu; wbinienda@uakron.edu; Robert.K.Goldberg@nasa.gov
NR 26
TC 13
Z9 13
U1 1
U2 10
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2011
VL 24
IS 2
BP 170
EP 180
DI 10.1061/(ASCE)AS.1943-5525.0000029
PG 11
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 752KU
UT WOS:000289690900006
ER
PT J
AU Keckhut, P
Randel, WJ
Claud, C
Leblanc, T
Steinbrecht, W
Funatsu, BM
Bencherif, H
McDermid, IS
Hauchecorne, A
Long, C
Lin, R
Baumgarten, G
AF Keckhut, P.
Randel, W. J.
Claud, C.
Leblanc, T.
Steinbrecht, W.
Funatsu, B. M.
Bencherif, H.
McDermid, I. S.
Hauchecorne, A.
Long, C.
Lin, R.
Baumgarten, G.
TI An evaluation of uncertainties in monitoring middle atmosphere
temperatures with the ground-based lidar network in support of space
observations
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Middle atmosphere temperature; Lidar; Satellite; Uncertainties
ID RESOLUTION DOPPLER IMAGER; LONG-TERM CHANGES; STRATOSPHERIC OZONE;
THERMAL TIDES; PART I; TRENDS; CLIMATOLOGY; ROCKETSONDES; VARIABILITY;
MESOSPHERE
AB The capability of the longest lidar data sets to monitor long-term temperature changes have been evaluated through comparisons with the successive Stratospheric Sounder Units (SSU) onboard NOAA satellites. Cross-consistency investigations between SSU and the lidar network can be considered as a first attempt to demonstrate how the synergistic use of space and ground-based instruments could provide reliable monitoring of the temperature of the middle atmosphere. The breakdown of the temperature cooling trend, and the following flattening observed in the satellite temperature series, is qualitatively confirmed by the lidars. However, there are still large differences that can either be due to SSU continuity (orbit drifts or weighting function modifications) or lidar operation changes (time of measurements, accuracy, sampling, etc.). SSU vertical weighting functions have been taken into account for comparisons. Some discontinuity events cannot be explained by the SSU weighting function drifts due to CO(2). For the upper channels of SSU (peaking around 50 km), the results are probably sensitive to the mesospheric part of the lidar profiles that can explain some discontinuities. Tropical lidar stations show clear inter-annual differences with the SSU channels covering the lowest altitude range that needs further investigations to understand if the origin is instrumental or geophysical. An attempt to derive non-linear trends with combinations of linear, hockey stick, and quadratic functions has been made. While the quadratic term is not highly significant, this approach allows the derivation of a better quantification of the linear trend terms. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Keckhut, P.; Funatsu, B. M.; Hauchecorne, A.] Univ Versailles St Quentin 11, Lab Atmospheres, UMR 8190, Inst Pierre Simon Laplace, F-78280 Verrieres Le Buisson, France.
[Randel, W. J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Claud, C.; Funatsu, B. M.] Ecole Polytech, Meteorol Dynam Lab, UMR 8539, Inst Pierre Simon Laplace, F-91128 Palaiseau, France.
[Leblanc, T.; McDermid, I. S.] CALTECH, Jet Prop Lab, Wrightwood, CA USA.
[Steinbrecht, W.] Meteorol Observ, Hohenpeissenberg, Germany.
[Bencherif, H.] Univ La Reunion, Lab Atmosphere & Cyclones, UMR 8105, St Denis, France.
[Long, C.; Lin, R.] NOAA, Predict Ctr, NCEP, Natl Weather Serv, Camp Springs, MD USA.
[Baumgarten, G.] Leibniz Inst Atmospher Phys, Kuhlungsborn, Germany.
RP Keckhut, P (reprint author), Univ Versailles St Quentin 11, Lab Atmospheres, UMR 8190, Inst Pierre Simon Laplace, Blvd Alembert, F-78280 Verrieres Le Buisson, France.
EM Keckhut@latmos.ipsl.fr
RI Steinbrecht, Wolfgang/G-6113-2010; Hauchecorne, Alain/A-8489-2013;
Randel, William/K-3267-2016;
OI Steinbrecht, Wolfgang/0000-0003-0680-6729; Randel,
William/0000-0002-5999-7162; Claud, Chantal/0000-0001-7613-9525;
Hauchecorne, Alain/0000-0001-9888-6994; Baumgarten,
Gerd/0000-0002-6727-284X
FU COST Action [ES0702]; European Commission [FP6-2005-Global-4-036677]
FX This work was initiated through the SPARC Stratospheric Temperature
Trend Assessment group lead by Dr. W. Randel
(http://www.atmosp.physics.utoronto.ca/SPARC/initiatives
NEW2005Detection.html) and was partly supported by the European
Commission through the Global Earth Observation and Monitoring
(GEOmon-http://www.geomon.eu/) Integrated Project under the 6th
Framework Program (Contract no. FP6-2005-Global-4-036677). It is also
part of the COST Action ES0702: European Ground-Based Observations of
Essential Variables for Climate and Operational Meteorology (EG-CLIMET).
NR 52
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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 APR
PY 2011
VL 73
IS 5-6
BP 627
EP 642
DI 10.1016/j.jastp.2011.01.003
PG 16
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 741UC
UT WOS:000288889600008
ER
PT J
AU Gopalswamy, N
Davila, JM
St Cyr, OC
Sittler, EC
Auchere, F
Duvall, TL
Hoeksema, JT
Maksimovic, M
MacDowall, RJ
Szabo, A
Collier, MR
AF Gopalswamy, N.
Davila, J. M.
St Cyr, O. C.
Sittler, E. C.
Auchere, F.
Duvall, T. L., Jr.
Hoeksema, J. T.
Maksimovic, M.
MacDowall, R. J.
Szabo, A.
Collier, M. R.
TI Earth-Affecting Solar Causes Observatory (EASCO): A potential
International Living with a Star Mission from Sun-Earth L5
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article; Proceedings Paper
CT Meeting on International Living With a Star (ILWS)
CY OCT 04-09, 2009
CL Ubatuba, BRAZIL
DE Coronal mass ejections; Earth-Sun L5; Corotating interaction regions;
Geomagnetic storms; Solar energetic particles
ID CORONAL MASS EJECTIONS; II RADIO-BURSTS; GEOMAGNETIC STORMS; SPACE
AB This paper describes the scientific rationale for an L5 mission and a partial list of key scientific instruments the mission should carry. The L5 vantage point provides an unprecedented view of the solar disturbances and their solar sources that can greatly advance the science behind space weather. A coronagraph and a heliospheric imager at L5 will be able to view CMEs broadsided, so space speed of the Earth-directed CMEs can be measured accurately and their radial structure discerned. In addition, an inner coronal imager and a magnetograph from L5 can give advance information on active regions and coronal holes that will soon rotate on to the solar disk. Radio remote sensing at low frequencies can provide information on shock-driving CMEs, the most dangerous of all CMEs. Coordinated helioseismic measurements from the Sun-Earth line and L5 provide information on the physical conditions at the base of the convection zone, where solar magnetism originates. Finally, in situ measurements at L5 can provide information on the large-scale solar wind structures (corotating interaction regions (CIRs)) heading towards Earth that potentially result in adverse space weather. Published by Elsevier Ltd.
C1 [Gopalswamy, N.; Davila, J. M.; St Cyr, O. C.; Sittler, E. C.; Duvall, T. L., Jr.; MacDowall, R. J.; Szabo, A.; Collier, M. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Auchere, F.] Inst Astrophys Spatiale, Orsay, France.
[Hoeksema, J. T.] Stanford Univ, Stanford, CA 94305 USA.
[Maksimovic, M.] Observ Paris, Meudon, France.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM nat.gopalswamy@nasa.gov
RI Duvall, Thomas/C-9998-2012; MacDowall, Robert/D-2773-2012; Gopalswamy,
Nat/D-3659-2012; Collier, Michael/I-4864-2013;
OI Collier, Michael/0000-0001-9658-6605; Auchere,
Frederic/0000-0003-0972-7022
NR 21
TC 18
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U1 0
U2 5
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 APR
PY 2011
VL 73
IS 5-6
BP 658
EP 663
DI 10.1016/j.jastp.2011.01.013
PG 6
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 741UC
UT WOS:000288889600011
ER
PT J
AU Tsurutani, BT
Lakhina, GS
Verkhoglyadova, OP
Gonzalez, WD
Echer, E
Guarnieri, FL
AF Tsurutani, B. T.
Lakhina, G. S.
Verkhoglyadova, O. P.
Gonzalez, W. D.
Echer, E.
Guarnieri, F. L.
TI A review of interplanetary discontinuities and their geomagnetic effects
(vol 73, pg 5, 2011)
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Correction
C1 [Tsurutani, B. T.; Verkhoglyadova, O. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Lakhina, G. S.] Indian Inst Geomagnetism, Navi Mumbai, India.
[Verkhoglyadova, O. P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Gonzalez, W. D.; Echer, E.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, SP, Brazil.
[Guarnieri, F. L.] Univ Vale do Paraiba, Sao Jose Dos Campos, SP, Brazil.
RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM bruce.tsurutani@jpl.nasa.gov
RI Lakhina, Gurbax /C-9295-2012; Tecnologias espaciai, Inct/I-2415-2013
NR 3
TC 0
Z9 0
U1 0
U2 2
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 APR
PY 2011
VL 73
IS 5-6
BP 709
EP 709
DI 10.1016/j.jastp.2011.01.007
PG 1
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 741UC
UT WOS:000288889600017
ER
PT J
AU Lyver, JW
Blaisten-Barojas, E
AF Lyver, John W.
Blaisten-Barojas, Estela
TI Lattice Thermal Conductivity in SiC Nanotubes, Nanowires and
Nanofilaments: A Molecular Dynamics Study
SO JOURNAL OF COMPUTATIONAL AND THEORETICAL NANOSCIENCE
LA English
DT Article
DE Thermal Conductivity; Non-Equilibrium Molecular Dynamics; Silicon
Carbide; SiC Nanowires; SiC Nanotubes; SiC Nanofilaments
ID FINITE-TEMPERATURE PROPERTIES; SILICON-CARBIDE; HEAT-FLOW; SIMULATIONS;
TRANSPORT; CRYSTALS; WALL
AB This paper presents results a non-equilibrium Molecular Dynamics approach to determine the lattice thermal conductivity of nanowires, nanotubes, and nanofilaments of silicon carbide. The nanostructures are modeled with the classical potential proposed in J Appl. Phys. 101, 103515 (2007). These nanostructures display very low lattice thermal conductivity, about 50 times smaller than bulk SiC. Among the studied nanostructures, the 3C [(1) over bar 00] nanowires have the highest thermal conductivity, and the (5, 5) nanotubes display the lowest. Dependence on temperature of the lattice thermal conductivity exhibits an inverse power relationship only for nanowires 3C [(1) over bar 00], 2H [110] and the (4, 0), (2, 2) nanotubes. All other structures have thermal conductivities decreasing more gently as a function of increasing temperature, except for nanowires 3C and nanotubes (5, 5) where the thermal conductivity is almost constant as a function of temperature.
C1 [Lyver, John W.; Blaisten-Barojas, Estela] George Mason Univ, Computat Mat Sci Ctr, Fairfax, VA 22030 USA.
[Lyver, John W.; Blaisten-Barojas, Estela] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Lyver, John W.] NASA, Off Safety & Mission Assurance, Washington, DC 20546 USA.
RP Blaisten-Barojas, E (reprint author), George Mason Univ, Computat Mat Sci Ctr, MS 6A2, Fairfax, VA 22030 USA.
FU National Science Foundation [CHE-0626111]
FX This work was supported in part by the National Science Foundation,
grant CHE-0626111.
NR 32
TC 7
Z9 7
U1 0
U2 8
PU AMER SCIENTIFIC PUBLISHERS
PI STEVENSON RANCH
PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA
SN 1546-1955
J9 J COMPUT THEOR NANOS
JI J. Comput. Theor. Nanosci.
PD APR
PY 2011
VL 8
IS 4
BP 529
EP 534
DI 10.1166/jctn.2011.1718
PG 6
WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials
Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA 752NH
UT WOS:000289698200002
ER
PT J
AU Palof, KJ
Heifetz, J
Gharrett, AJ
AF Palof, Katie J.
Heifetz, Jonathan
Gharrett, Anthony J.
TI Geographic structure in Alaskan Pacific ocean perch (Sebastes alutus)
indicates limited lifetime dispersal
SO MARINE BIOLOGY
LA English
DT Article
ID EFFECTIVE POPULATION-SIZE; MULTILOCUS GENOTYPE DATA; QUEEN-CHARLOTTE
SOUND; ROCKFISH SEBASTES; GENE FLOW; MICROSATELLITE LOCI; F-STATISTICS;
LINKAGE DISEQUILIBRIUM; PAIRWISE RELATEDNESS; ALLELE FREQUENCIES
AB Prevailing oceanographic processes, pelagic larvae, adult mobility, and large populations of many marine species often leads to the assumption of wide-ranging populations. Applying this assumption to more localized populations can lead to inappropriate conservation measures. The Pacific ocean perch (Sebastes alutus, POP) is economically and ecologically valuable, but little is known about its population structure and life history in Alaskan waters. Fourteen microsatellite loci were used to characterize geographic structure and connectivity of POP collections (1999-2005) sampled along the continental shelf break from Dixon Entrance to the Bering Sea. Despite opportunities for dispersal, there was significant, geographically related genetic structure (F(ST) = 0.0123, P < 10(-5)). Adults appear to belong to neighborhoods at geographic scales less than 400 km, and possibly as small as 70 km, which indicates limited dispersal throughout their lives. The population structure observed has a finer geographic scale than current management, which suggests that measures for POP fisheries conservation should be revisited.
C1 [Palof, Katie J.; Gharrett, Anthony J.] Univ Alaska Fairbanks, Div Fisheries, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
[Heifetz, Jonathan] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, NOAA, Juneau, AK 99801 USA.
RP Palof, KJ (reprint author), Univ Alaska Fairbanks, Div Fisheries, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM kjpalof@alaska.edu
FU Alaska Sea Grant College Program; Cooperative Institute for Artic
Research (CIFAR); NOAA Fisheries-Auke Bay Laboratories; Rasmuson
Fisheries Research Center; Pollock Conservation Cooperative Research
Center (PCCRC); School of Fisheries and Ocean Sciences, University of
Alaska Fairbanks, AK
FX We thank R. Waples and L. Hauser for their helpful comments and review.
We thank N. Hillgruber for serving on the graduate committee and for her
helpful comments. We thank Alaska Fisheries Science Center, NOAA
Fisheries personnel who took tissue samples for this study during trawl
surveys. This research was supported by: Alaska Sea Grant College
Program, Cooperative Institute for Artic Research (CIFAR), NOAA
Fisheries-Auke Bay Laboratories, Rasmuson Fisheries Research Center, and
the Pollock Conservation Cooperative Research Center (PCCRC), School of
Fisheries and Ocean Sciences, University of Alaska Fairbanks, AK. This
work represents, in part, the master's work of K. Palof at the
University of Alaska Fairbanks.
NR 82
TC 13
Z9 13
U1 0
U2 10
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0025-3162
J9 MAR BIOL
JI Mar. Biol.
PD APR
PY 2011
VL 158
IS 4
BP 779
EP 792
DI 10.1007/s00227-010-1606-2
PG 14
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 750IF
UT WOS:000289539100007
ER
PT J
AU Hochhalter, JD
Littlewood, DJ
Veilleux, MG
Bozek, JE
Maniatty, AM
Rollett, AD
Ingraffea, AR
AF Hochhalter, J. D.
Littlewood, D. J.
Veilleux, M. G.
Bozek, J. E.
Maniatty, A. M.
Rollett, A. D.
Ingraffea, A. R.
TI A geometric approach to modeling microstructurally small fatigue crack
formation: III. Development of a semi-empirical model for nucleation
SO MODELLING AND SIMULATION IN MATERIALS SCIENCE AND ENGINEERING
LA English
DT Article
ID POLYCRYSTAL PLASTICITY; ALUMINUM-ALLOY; CYCLE FATIGUE; GROWTH;
DISLOCATION
AB It has been observed during fatigue cracking of AA 7075-T651 that a small percentage of Al(7)Cu(2)Fe particles crack during manufacturing or very early in their life. Some of the cracked particles eventually nucleate cracks into the surrounding microstructure, and among these the number of cycles required for nucleation varies widely. It is important to comprehend the mechanics underpinning the observed variation so that the subsequent propagation stage can be accurately modeled. To this end, finite element models of replicated grain and particle geometry are used to compute mechanical fields near monitored cracked particles using an elastic-viscoplastic crystal plasticity model that captures the effect of the orientation of the grains near each monitored particle. Nonlocal, slip-based metrics are used to study the localization and cyclic accumulation of slip near the cracked particles providing mechanics-based insight into the actuation of the nucleation event. A high slip localization and cyclic accumulation rate are found to be a necessary, but not sufficient, condition for nucleation from cracked particles. A sufficient local driving stress must also be present, which is strongly dependent on the local microstructure and accumulated slip. Furthermore, the simulation results elucidate a quantitative relationship between the slip accumulated during fatigue loading and a consequential reduction of the critical local driving stress for nucleation, providing a physical basis for the fatigue damage concept. The observed nucleation direction is orthogonal to the computed local maximum tangential stress direction, as expected for this alloy. The main result is a semi-empirical model for the number of cycles required for nucleation, which is dependent on the maximum tangential stress and cyclic slip-accumulation rate near a cracked particle.
C1 [Hochhalter, J. D.] NASA, Durabil & Damage Tolerance Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Littlewood, D. J.] Sandia Natl Labs, Albuquerque, NM 87185 USA.
[Veilleux, M. G.; Bozek, J. E.; Ingraffea, A. R.] Cornell Univ, Cornell Fracture Grp, Ithaca, NY 14853 USA.
[Maniatty, A. M.] Rensselaer Polytech Inst, Troy, NY 12180 USA.
[Rollett, A. D.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA.
RP Hochhalter, JD (reprint author), NASA, Durabil & Damage Tolerance Branch, Langley Res Ctr, MS 188E, Hampton, VA 23681 USA.
EM Jacob.D.Hochhalter@nasa.gov
RI Rollett, Anthony/A-4096-2012
OI Rollett, Anthony/0000-0003-4445-2191
FU Defense Advanced Research Projects Agency (DARPA) [HR0011-04-C-0003];
NASA [ARMD-NNX07AB69A]; NASA Advanced Supercomputing Division at Ames
Research Center
FX Dr Gerd Heber developed the parallel finite element code that was used
for the finite element simulations presented here. The measurements of
microstructural geometry were made by Robert Christ Jr and Dr Elias
Anagnostou at the Northrop Grumman Corporation. This work is partially
sponsored by the Defense Advanced Research Projects Agency (DARPA) under
contract HR0011-04-C-0003. Dr Leo Christodoulou is the DARPA Program
Manager. This work is also partially funded by NASA under contract
ARMD-NNX07AB69A. Dr Ed Glaessgen is the National Aeronautics and Space
Administration (NASA) Contract Monitor. Resources supporting this work
were provided by the NASA High-End Computing Program through the NASA
Advanced Supercomputing Division at Ames Research Center. The views,
opinions, and/or findings contained in this paper are those of the
authors and should not be interpreted as representing the official views
or policies, either expressed or implied, of the Defense Advanced
Research Projects Agency or the Department of Defense.
NR 23
TC 11
Z9 11
U1 1
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0965-0393
J9 MODEL SIMUL MATER SC
JI Model. Simul. Mater. Sci. Eng.
PD APR
PY 2011
VL 19
IS 3
AR 035008
DI 10.1088/0965-0393/19/3/035008
PG 27
WC Materials Science, Multidisciplinary; Physics, Applied
SC Materials Science; Physics
GA 753MG
UT WOS:000289778700008
ER
PT J
AU Guo, Q
Cole, S
Lacey, CG
Baugh, CM
Frenk, CS
Norberg, P
Auld, R
Baldry, IK
Bamford, SP
Bourne, N
Buttiglione, ES
Cava, A
Cooray, A
Croom, S
Dariush, A
De Zotti, G
Driver, S
Dunne, L
Dye, S
Eales, S
Fritz, J
Hopkins, A
Hopwood, R
Ibar, E
Ivison, RJ
Jarvis, M
Jones, DH
Kelvin, L
Liske, J
Loveday, J
Maddox, SJ
Parkinson, H
Pascale, E
Peacock, JA
Pohlen, M
Prescott, M
Rigby, EE
Robotham, A
Rodighiero, G
Sharp, R
Smith, DJB
Temi, P
van Kampen, E
AF Guo, Qi
Cole, Shaun
Lacey, Cedric G.
Baugh, Carlton M.
Frenk, Carlos S.
Norberg, Peder
Auld, R.
Baldry, I. K.
Bamford, S. P.
Bourne, N.
Buttiglione, E. S.
Cava, A.
Cooray, A.
Croom, S.
Dariush, A.
De Zotti, G.
Driver, S.
Dunne, L.
Dye, S.
Eales, S.
Fritz, J.
Hopkins, A.
Hopwood, R.
Ibar, E.
Ivison, R. J.
Jarvis, M.
Jones, D. H.
Kelvin, L.
Liske, J.
Loveday, J.
Maddox, S. J.
Parkinson, H.
Pascale, E.
Peacock, J. A.
Pohlen, M.
Prescott, M.
Rigby, E. E.
Robotham, A.
Rodighiero, G.
Sharp, R.
Smith, D. J. B.
Temi, P.
van Kampen, E.
TI Which haloes host Herschel-ATLAS galaxies in the local Universe?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: haloes; dark matter; infrared: galaxies
ID STAR-FORMATION HISTORY; LOW-REDSHIFT UNIVERSE; MASS ASSEMBLY GAMA;
DARK-MATTER; LUMINOSITY FUNCTION; FORMING GALAXIES; FORMATION RATES;
NUMBER; SPIRE; BIAS
AB We measure the projected cross-correlation between low-redshift (z < 0.5) far-infrared selected galaxies in the science demonstration phase (SDP) field of the Herschel-ATLAS (H-ATLAS) survey and optically selected galaxies from the Galaxy and Mass Assembly (GAMA) redshift survey. In order to obtain robust correlation functions, we restrict the analysis to a subset of 969 out of 6900 H-ATLAS galaxies, which have reliable optical counterparts with r < 19.4 mag and well-determined spectroscopic redshifts. The overlap region between the two surveys is 12.6 deg2; the matched sample has a median redshift of z approximate to 0.2. The cross-correlation of GAMA and H-ATLAS galaxies within this region can be fitted by a power law, with correlation length r(0) approximate to 4.63 +/- 0.51 Mpc. Comparing with the corresponding autocorrelation function of GAMA galaxies within the SDP field yields a relative bias (averaged over 2-8 Mpc) of H-ATLAS and GAMA galaxies of b(H)/b(G) approximate to 0.6. Combined with clustering measurements from previous optical studies, this indicates that most of the low-redshift H-ATLAS sources are hosted by haloes with masses comparable to that of the Milky Way. The correlation function appears to depend on the 250-mu m luminosity, L-250, with bright (median luminosity nu L-250 similar to 1.6 x 1010 L-circle dot) objects being somewhat more strongly clustered than faint (nu L-250 similar to 4.0 x 109 L-circle dot) objects. This implies that galaxies with higher dust-obscured star formation rates are hosted by more massive haloes.
C1 [Norberg, Peder; Parkinson, H.; Peacock, J. A.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Pascale, E.; Pohlen, M.; Smith, D. J. B.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales.
[Baldry, I. K.; Prescott, M.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Bamford, S. P.; Bourne, N.; Dunne, L.; Maddox, S. J.; Rigby, E. E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Buttiglione, E. S.; De Zotti, G.; Rodighiero, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Cava, A.] Inst Astrofis Canarias IAC, Tenerife, Spain.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Croom, S.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia.
[De Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Driver, S.; Kelvin, L.; Robotham, A.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Fritz, J.] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium.
[Hopkins, A.; Jones, D. H.; Sharp, R.] Australian Astron Observ, Epping, NSW 1710, Australia.
[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.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England.
[Liske, J.; van Kampen, E.] European So Observ, D-85748 Garching, Germany.
[Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Guo, Qi; Cole, Shaun; Lacey, Cedric G.; Baugh, Carlton M.; Frenk, Carlos S.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Cava, A.] Dept Astrofis La Laguna ULL, Tenerife, Spain.
RP Guo, Q (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England.
EM qi.guo@durham.ac.uk
RI Baugh, Carlton/A-8482-2012; Robotham, Aaron/H-5733-2014; Driver,
Simon/H-9115-2014; Ivison, R./G-4450-2011; Bamford, Steven/E-8702-2010;
Cava, Antonio/C-5274-2017;
OI Rodighiero, Giulia/0000-0002-9415-2296; Liske,
Jochen/0000-0001-7542-2927; Baldry, Ivan/0000-0003-0719-9385; Dye,
Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X; Baugh,
Carlton/0000-0002-9935-9755; Robotham, Aaron/0000-0003-0429-3579;
Driver, Simon/0000-0001-9491-7327; Ivison, R./0000-0001-5118-1313;
Bamford, Steven/0000-0001-7821-7195; Cava, Antonio/0000-0002-4821-1275;
Maddox, Stephen/0000-0001-5549-195X
FU Royal Society; Leverhulme Research Fellowship; Science and Technology
Facilities Council; NASA through JPL
FX CSF acknowledges a Royal Society Wolfson Research Merit award. SC
acknowledges the support of the Leverhulme Research Fellowship. This
work was supported in part by a rolling grant from the Science and
Technology Facilities Council to the ICC. The H-ATLAS survey is being
carried with ESA's Herschel Space Observatory, which is equipped with
instruments provided by European-led Principal Investigator consortia,
with important participation from the NASA, USA. Authors acknowledge
support provided by the NASA through JPL. The GAMA is a joint
European-Australian spectroscopic campaign using the Anglo-Australian
Telescope. The GAMA input catalogue is based on data from the SDSS and
the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA
regions is being obtained by a number of independent surveys, including
GALEX MIS, VST KIDS, VISTA VIKING, WISE, H-ATLAS, GMRT and ASKAP,
providing UV to radio coverage. PN acknowledges the support of a Royal
Society University Research Fellowship. We thank Douglas Scott for a
critical reading of our manuscript.
NR 34
TC 13
Z9 13
U1 1
U2 4
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 APR
PY 2011
VL 412
IS 4
BP 2277
EP 2285
DI 10.1111/j.1365-2966.2010.18051.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 747BR
UT WOS:000289295800012
ER
PT J
AU De Sanctis, MC
Ammannito, E
Migliorini, A
Lazzaro, D
Capria, MT
McFadden, L
AF De Sanctis, Maria Cristina
Ammannito, Eleonora
Migliorini, Alessandra
Lazzaro, Daniela
Capria, Maria Teresa
McFadden, Lucy
TI Mineralogical characterization of some V-type asteroids, in support of
the NASA Dawn mission star
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE minor planets; asteroids general; minor planets; asteroids: individual:
4 Vesta
ID EUCRITE PARENT BODY; MAIN-BELT; BASALTIC ASTEROIDS; 4 VESTA; REFLECTANCE
SPECTRA; PYROXENE MIXTURES; SOLAR-SYSTEM; DIOGENITES; SPECTROSCOPY;
METEORITES
AB We present new reflectance spectra of 12 V-type asteroids obtained at the 3.6 m Telescopio Nazionale Galileo (TNG) covering the spectral range 0.7 to 2.5 mu m. This spectral range, encompassing the 1 and 2 mu m, pyroxene features, allows a precise mineralogical characterization of the asteroids. The spectra of these asteroids are examined and compared to spectra for the Howardite, Eucrite and Diogenite (HED) meteorites, of which Vesta is believed to be the parent body. The observed objects were selected from different dynamical populations with the aim to verify if there exist spectral parameters that can shed light on the origin of the objects. A reassessment of data previously published has also been performed using a new methodology. We derive spectral parameters from NIR spectra to infer mineralogical information of the observed asteroids.
The V-type asteroids here discussed show mainly orthopyroxene mineralogy although some of them seem to have a mineralogical composition containing cations that are smaller than Mg cations. Most of the observed Vestoids show a low abundance of Ca (< 10 per cent Wo). This result implies that no one of the Vestoids studied consists of just eucritic material, but they must additionally have a diogenitic component. However, we must remember that the ground-based data are subject to larger errors than the laboratory data used as reference spectra for interpretation.
Finally, we note that the intermediate belt asteroid (21238) 1995WV7 has spectral parameters quite different from the observed V-type objects of the inner belt, so it could be a basaltic asteroid not related to Vesta.
This mineralogical analysis of asteroids related to Vesta is done in support of NASA's Dawn mission, which will enter into orbit around Vesta in the summer of 2011. This work extends the scientific context of the mission to include processes contributing to the nature of smaller V-type asteroids that may be related to Vesta.
C1 [De Sanctis, Maria Cristina; Migliorini, Alessandra; Capria, Maria Teresa] Ist Astrofis Spaziale & Fis Cosm, Area Ric Tor Vergata, I-00133 Rome, Italy.
[Ammannito, Eleonora] Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy.
[Lazzaro, Daniela] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[McFadden, Lucy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP De Sanctis, MC (reprint author), Ist Astrofis Spaziale & Fis Cosm, Area Ric Tor Vergata, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM mariacristina.desanctis@iasf-roma.inaf.it
RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; McFadden,
Lucy-Ann/I-4902-2013; De Sanctis, Maria Cristina/G-5232-2013; Lazzaro,
Daniela/I-3509-2012;
OI McFadden, Lucy-Ann/0000-0002-0537-9975; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Lazzaro, Daniela/0000-0002-4470-6043;
Migliorini, Alessandra/0000-0001-7386-9215; capria, maria
teresa/0000-0002-9814-9588
FU ASI
FX This work has been supported by an ASI grant, whose support is
gratefully acknowledged.
NR 65
TC 17
Z9 17
U1 1
U2 4
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 APR
PY 2011
VL 412
IS 4
BP 2318
EP 2332
DI 10.1111/j.1365-2966.2010.18058.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 747BR
UT WOS:000289295800015
ER
PT J
AU Dudek, JC
AF Dudek, Julianne C.
TI Modeling Vortex Generators in a Navier-Stokes Code
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 48th AIAA Aerospace Sciences Meeting and Exhibit Including the New
Horizons Forum and Aerospace Exposition
CY JAN 04-08, 2010
CL Orlando, FL
SP AIAA, Vinnova, Maritime Competence Ctr Lighthouse, Swedish Armed Forces, Swedish Def Mat Agcy, NASA Langley Res Ctr, NASA Dryden Flight Res Ctr
AB A source-term model that simulates the effects of vortex generators was implemented into the Wind-US Navier- Stokes code. The source term added to the Navier-Stokes equations simulates the lift force that would result from a vane-type vortex generator in the flowfield. The implementation is user-friendly, requiring the user to specify only three quantities for each desired vortex generator: the range of grid points over which the force is to be applied and the planform area and angle of incidence of the physical vane. The model behavior was evaluated for subsonic flow in a rectangular duct with a single vane vortex generator, subsonic flow in an S-duct with 22 corotating vortex generators, and supersonic flow in a rectangular duct with a counter-rotating vortex-generator pair. The model was also used to successfully simulate microramps in supersonic flow by treating each microramp as a pair of vanes with opposite angles of incidence. The validation results indicate that the source-term vortex-generator model provides a useful tool for screening vortex-generator configurations and gives comparable results to solutions computed using gridded vanes.
C1 NASA John H Glenn Res Ctr Lewis Field, Inlet & Nozzle Branch, Cleveland, OH 44135 USA.
RP Dudek, JC (reprint author), NASA John H Glenn Res Ctr Lewis Field, Inlet & Nozzle Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
NR 16
TC 7
Z9 7
U1 1
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD APR
PY 2011
VL 49
IS 4
BP 748
EP 759
DI 10.2514/1.J050683
PG 12
WC Engineering, Aerospace
SC Engineering
GA 745SI
UT WOS:000289185800007
ER
PT J
AU Diskin, B
Thomas, JL
AF Diskin, Boris
Thomas, James L.
TI Comparison of Node-Centered and Cell-Centered Unstructured Finite Volume
Discretizations: Inviscid Fluxes
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 48th AIAA Aerospace Sciences Meeting/New Horizons Forum and Aerospace
Exposition
CY JAN 04-08, 2010
CL Orlando, FL
SP AIAA
ID SOLVERS
AB Nominally second-order cell-centered and node-centered approaches are compared for unstructured finite volume discretization of inviscid fluxes in two dimensions. Three classes of grids are considered: isotropic grids in a rectangular geometry, anisotropic grids typical of adapted grids, and anisotropic grids over a curved surface typical of advancing-layer grids. The classes contain regular and irregular grids, including mixed-element grids and grids with random perturbations of nodes. Complexity, accuracy, and convergence of defect-correction iterations are studied. Deficiencies of specific schemes, such as instability, accuracy degradation, and/or poor convergence of defect-correction iterations, have been observed in computations and confirmed in analysis. All schemes may produce large relative gradient-reconstruction errors on grids with perturbed nodes. On advancing-layer grids, a local approximate-mapping technique based on the distance function restores gradient-reconstruction accuracy and fast convergence of defect-correction iterations. Among the considered scheme, the best cell-centered and node-centered schemes, which are low-complexity, stable, robust, and uniformly second-order-accurate, are recommended.
C1 [Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23681 USA.
[Diskin, Boris] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
[Thomas, James L.] NASA, Langley Res Ctr, AeroSci Branch, Hampton, VA 23681 USA.
RP Diskin, B (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23681 USA.
EM bdiskin@nianet.org; james.l.thomas@nasa.gov
NR 21
TC 7
Z9 9
U1 0
U2 4
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD APR
PY 2011
VL 49
IS 4
BP 836
EP 854
DI 10.2514/1.J050897
PG 19
WC Engineering, Aerospace
SC Engineering
GA 745SI
UT WOS:000289185800014
ER
PT J
AU Samanta, A
Appelo, D
Colonius, T
Nott, J
Hall, J
AF Samanta, Arnab
Appeloe, Daniel
Colonius, Tim
Nott, Julian
Hall, Jeffrey
TI Comment on "Computational Modeling and Experiments of Natural Convection
for a Titan Montgolfiere" Reply
SO AIAA JOURNAL
LA English
DT Editorial Material
ID SPHERES
C1 [Samanta, Arnab; Colonius, Tim] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[Nott, Julian] Nott Technol LLC, Santa Barbara, CA 93101 USA.
[Hall, Jeffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
RP Samanta, A (reprint author), CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
NR 7
TC 1
Z9 1
U1 0
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD APR
PY 2011
VL 49
IS 4
BP 877
EP 878
DI 10.2514/1.J050961
PG 2
WC Engineering, Aerospace
SC Engineering
GA 745SI
UT WOS:000289185800019
ER
PT J
AU Barnes, NP
Amzajerdian, F
Reichle, DJ
Carrion, WA
Busch, GE
Leisher, P
AF Barnes, N. P.
Amzajerdian, F.
Reichle, D. J.
Carrion, W. A.
Busch, G. E.
Leisher, P.
TI Diode pumped Ho:YAG and Ho:LuAG lasers, Q-switching and second harmonic
generation
SO APPLIED PHYSICS B-LASERS AND OPTICS
LA English
DT Article
ID HO-YAG LASER; TM-YLF LASER; ROOM-TEMPERATURE; OPERATION; EMISSION
AB Direct diode pumped Ho:YAG generated laser pulses at 2.12 mu m with an optical to optical slope efficiency of 0.24. Ho:YAG and Ho:LuAG laser rods were evaluated with both wide and narrow bandwidth pump diodes. The laser wavelength varies with the level of pumping and optical design. This variation was found to be predictable. Second harmonic at 1.06 mu m was produced in a 6.0 mm long BBO crystal.
C1 [Barnes, N. P.; Amzajerdian, F.; Reichle, D. J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Carrion, W. A.; Busch, G. E.] Coherent Applicat Inc, Hampton, VA 23681 USA.
[Leisher, P.] nLight, Vancouver, WA 98665 USA.
RP Barnes, NP (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM norman.p.barnes@nasa.gov
NR 22
TC 16
Z9 16
U1 5
U2 29
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0946-2171
EI 1432-0649
J9 APPL PHYS B-LASERS O
JI Appl. Phys. B-Lasers Opt.
PD APR
PY 2011
VL 103
IS 1
BP 57
EP 66
DI 10.1007/s00340-010-4195-3
PG 10
WC Optics; Physics, Applied
SC Optics; Physics
GA 750OY
UT WOS:000289559000011
ER
PT J
AU Cao, H
Russell, CT
Christensen, UR
Dougherty, MK
Burton, ME
AF Cao, Hao
Russell, Christopher T.
Christensen, Ulrich R.
Dougherty, Michele K.
Burton, Marcia E.
TI Saturn's very axisymmetric magnetic field: No detectable secular
variation or tilt
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Saturn; magnetic dynamo; interior structure
ID ROTATION PERIOD; PLANETS; DYNAMO; MODEL
AB Saturn is the only planet in the solar system whose observed magnetic field is highly axisymmetric. At least a small deviation from perfect symmetry is required for a dynamo-generated magnetic field. Analyzing more than six years of magnetometer data obtained by Cassini close to the planet, we show that Saturn's observed field is much more axisymmetric than previously thought. We invert the magnetometer observations that were obtained in the "current-free" inner magnetosphere for an internal model, varying the assumed unknown rotation rate of Saturn's deep interior. No unambiguous non-axially symmetric magnetic moment is detected, with a new upper bound on the dipole tilt of 0.06 degrees. An axisymmetric internal model with Schmidt-normalized spherical harmonic coefficients g10 = 21,191 +/- 24 nT, g20 = 1586 +/- 7 nT. g30 = 2374 +/- 47 nT is derived from these measurements, the upper bounds on the axial degree 4 and 5 terms are 720 nT and 3200 nT respectively. The secular variation for the last 30 years is within the probable error of each term from degree 1 to 3, and the upper bounds are an order of magnitude smaller than in similar terrestrial terms for degrees 1 and 2. Differentially rotating conducting stable layers above Saturn's dynamo region have been proposed to symmetrize the magnetic field (Stevenson, 1982). The new upper bound on the dipole tilt implies that this stable layer must have a thickness L >= 4000 km, and this thickness is consistent with our weak secular variation observations. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Cao, Hao; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Christensen, Ulrich R.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Dougherty, Michele K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Burton, Marcia E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cao, H (reprint author), 595 Charles E Young Dr E,6862 Slichter Hall, Los Angeles, CA 90095 USA.
EM haocao@ucla.edu
RI Cao, Hao/B-5689-2012;
OI Russell, Christopher/0000-0003-1639-8298
FU National Aeronautics and Space Administration [1236948]
FX This work at UCLA is supported by the National Aeronautics and Space
Administration under JPL contract 1236948. We thank the two reviewers
for their valuable comments and suggestions, which greatly improved this
paper.
NR 30
TC 18
Z9 18
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD APR 1
PY 2011
VL 304
IS 1-2
BP 22
EP 28
DI 10.1016/j.epsl.2011.02.035
PG 7
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 748KB
UT WOS:000289388400003
ER
PT J
AU Righter, K
AF Righter, K.
TI Prediction of metal-silicate partition coefficients for siderophile
elements: An update and assessment of PT conditions for metal-silicate
equilibrium during accretion of the Earth
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE mantle; siderophile; core formation; accretion; magma ocean
ID TERRESTRIAL MAGMA OCEAN; CORE FORMATION; OXYGEN FUGACITY; HIGH-PRESSURE;
OXIDATION-STATE; LOWER-MANTLE; MELT COMPOSITION; EXPERIMENTAL
CONSTRAINTS; CHEMICAL-COMPOSITION; TEMPERATURE
AB Experimental studies of the partitioning of siderophile elements between metallic and silicate liquids have provided fundamental constraints on the early history and differentiation conditions of the Earth. With many new studies even in the last 20 yr, several models have emerged from the results, including low pressure equilibrium, high pressure equilibrium, and combined high and low pressure multi-stage models. The reasons silicate melt composition, pressure effects on silicate melt structure, different methods for calculating metal activity coefficients, and the role of deep mantle phases - for the multitude of resulting models have not been specifically addressed before, yet are critical in evaluating the more likely and realistic models. The four reasons - leading to the divergence of results will be discussed and evaluated. The behavior of the moderately siderophile elements Ni and Co will be compared using several approaches, each of which results in the same conclusion for Ni and Co. This consistency will eliminate the supposition that one or the other approaches gives a more accurate answer for element partitioning. Newly updated expressions for 11 elements are then derived and presented and applied to the early Earth to evaluate the idea of a late stage equilibration between a core forming metal and silicate melt (or magma ocean). It is possible to explain all 11 elements at conditions of 27-33 GPa, 3300-3600 K, Delta IW = -1, for peridotite and a metallic liquid containing 10% of a light element. The main difference between the current result and several other recent modeling efforts is that Mn, V, and Cr are hosted in deep mantle phases as well as the core. The other elements - Ni, Co, Mo, W. P, Cu, Ga, and Pd - are hosted in core, and detailed modeling here shows the importance of accounting for oxygen fugacity, silicate and metallic liquid compositions, as well as temperature and pressure. The idea of late stage metal-silicate equilibrium at a restricted pressure and temperature range leaving a chemical finger print on the upper mantle remains viable. Published by Elsevier B.V.
C1 NASA Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA.
RP Righter, K (reprint author), NASA Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
FU RTOP from the NASA
FX B. Wood provided the Metalcalc code for calculating activity
coefficients for trace elements in metallic liquids. K. Leung and B.
Fessler provided computing assistance at the Lunar and Planetary
Institute. Discussions with L. Danielson, M. Humayun, A. Campbell, and
G. Shofner have been influential in the presentation of this work.
Journal reviews of L. Burkemper and two anonymous reviewers, as well as
the comments of R. Carlson, led to significant improvements in the
presentation of this work. Research is supported by an RTOP to KR from
the NASA Cosmochemistry program.
NR 86
TC 62
Z9 63
U1 4
U2 35
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD APR 1
PY 2011
VL 304
IS 1-2
BP 158
EP 167
DI 10.1016/j.epsl.2011.01.028
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 748KB
UT WOS:000289388400017
ER
PT J
AU Russell, MJ
Lecakes, GD
Mandayam, S
Jensen, S
AF Russell, Michael J.
Lecakes, George D., Jr.
Mandayam, Shreekanth
Jensen, Scott
TI The "Intelligent" Valve: A Diagnostic Framework for Integrated
System-Health Management of a Rocket-Engine Test Stand
SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT
LA English
DT Article
DE Automated test and diagnostic systems; human-computer interface; virtual
measurement systems
ID SENSOR VALIDATION
AB Valves play a critical role in rocket-engine test stands because they are essential for the cryogen transport mechanisms that are vital to test operations. Sensors that are placed on valves monitor the pressure, temperature, flow rate, valve position, and any other features that are required for diagnosing their functionality. Integrated system-health management (ISHM) algorithms have been used to identify and evaluate anomalous operating conditions of systems and subsystems (e. g., valves and valve components) on complex structures, such as rocket test stands. In order for such algorithms to be useful, there is a need to develop realistic models for the most common and problem-prone elements. Furthermore, the user needs to be provided with efficient tools to explore the nature of the anomaly and its possible effects on the element, as well as its relationship to the overall system state. This paper presents the development of an intelligent-valve framework that is capable of tracking and visualizing events of the large linear actuator valve (LLAV) in order to detect anomalous conditions. The framework employs a combination of technologies, including a dynamic data exchange data-transfer protocol, autoassociative neural networks, empirical and physical models, and virtual-reality environments. The diagnostic procedure that is developed has the ability to be integrated into existing ISHM systems and can be used for assessing the integrity of rocket-engine test-stand components.
C1 [Russell, Michael J.; Lecakes, George D., Jr.; Mandayam, Shreekanth] Rowan Univ, Elect & Comp Engn Dept, Glassboro, NJ 08028 USA.
[Jensen, Scott] Natl Aeronaut & Space Adm, Stennis Space Ctr, MS 39529 USA.
RP Russell, MJ (reprint author), Rowan Univ, Elect & Comp Engn Dept, Glassboro, NJ 08028 USA.
EM shreek@rowan.edu
FU National Aeronautics and Space Administration (NASA) Stennis Space
Center [NNX08BA19A]; NASA [NNX08AV98H, NNX07AO92H]
FX Manuscript received May 27, 2010; revised August 13, 2010; accepted
October 5, 2010. Date of publication January 17, 2011; date of current
version March 8, 2011. This work was supported in part by the National
Aeronautics and Space Administration (NASA) Stennis Space Center under
Grant/Cooperative Agreement-NNX08BA19A and in part by the NASA Graduate
Student Researchers Program under Grants/Cooperative
Agreements-NNX08AV98H and NNX07AO92H. The Associate Editor coordinating
the review process for this paper was Dr. John Sheppard.
NR 23
TC 4
Z9 4
U1 1
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9456
EI 1557-9662
J9 IEEE T INSTRUM MEAS
JI IEEE Trans. Instrum. Meas.
PD APR
PY 2011
VL 60
IS 4
BP 1489
EP 1497
DI 10.1109/TIM.2010.2101350
PG 9
WC Engineering, Electrical & Electronic; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 746AJ
UT WOS:000289212900040
ER
PT J
AU Goossens, S
Matsumoto, K
Liu, Q
Kikuchi, F
Sato, K
Hanada, H
Ishihara, Y
Noda, H
Kawano, N
Namiki, N
Iwata, T
Lemoine, FG
Rowlands, DD
Harada, Y
Chen, M
AF Goossens, S.
Matsumoto, K.
Liu, Q.
Kikuchi, F.
Sato, K.
Hanada, H.
Ishihara, Y.
Noda, H.
Kawano, N.
Namiki, N.
Iwata, T.
Lemoine, F. G.
Rowlands, D. D.
Harada, Y.
Chen, M.
TI Lunar gravity field determination using SELENE same-beam differential
VLBI tracking data
SO JOURNAL OF GEODESY
LA English
DT Article
DE Lunar gravity; Differential VLBI; Orbit determination; Gravity field
determination
ID BASE-LINE-INTERFEROMETRY; ORBIT DETERMINATION; PROSPECTOR; MISSION;
KAGUYA; VENUS; MOON; SIMULATION; SATELLITES; SELENODESY
AB A lunar gravity field model up to degree and order 100 in spherical harmonics, named SGM100i, has been determined from SELENE and historical tracking data, with an emphasis on using same-beam S-band differential VLBI data obtained in the SELENE mission between January 2008 and February 2009. Orbit consistency throughout the entire mission period of SELENE as determined from orbit overlaps for the two sub-satellites of SELENE involved in the VLBI tracking improved consistently from several hundreds of metres to several tens of metres by including differential VLBI data. Through orbits that are better determined, the gravity field model is also improved by including these data. Orbit determination performance for the new model shows improvements over earlier 100th degree and order models, especially for edge-on orbits over the deep far side. Lunar Prospector orbit determination shows an improvement of orbit consistency from 1-day predictions for 2-day arcs of 6 m in a total sense, with most improvement in the along and cross-track directions. Data fit for the types and satellites involved is also improved. Formal errors for the lower degrees are smaller, and the new model also shows increased correlations with topography over the far side. The estimated value for the lunar GM for this model equals 4902.80080 +/- 0.0009 km(3)/s(2) (10 sigma). The lunar degree 2 potential Love number k(2) was also estimated, and has a value of 0.0255 +/- 0.0016 (10 sigma as well).
C1 [Goossens, S.; Matsumoto, K.; Kikuchi, F.; Sato, K.; Hanada, H.; Ishihara, Y.; Noda, H.] Natl Astron Observ Japan, RISE Project, Oshu, Iwate 0230861, Japan.
[Liu, Q.; Kawano, N.; Harada, Y.; Chen, M.] Shanghai Astron Observ, Shanghai, Peoples R China.
[Namiki, N.] Chiba Inst Technol, Planetary Explorat Res Ctr, Chiba, Japan.
[Iwata, T.] Japan Aerosp Explorat Agcy, Kanagawa, Japan.
[Lemoine, F. G.; Rowlands, D. D.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Goossens, S (reprint author), Natl Astron Observ Japan, RISE Project, 2-12 Hoshigaoka, Oshu, Iwate 0230861, Japan.
EM sander@miz.nao.ac.jp
RI Rowlands, David/D-2751-2012; Ishihara, Yoshiaki/A-8499-2011; Lemoine,
Frank/D-1215-2013; he, shuyi/K-2082-2014; Goossens, Sander/K-2526-2015;
OI Goossens, Sander/0000-0002-7707-1128; Ishihara,
Yoshiaki/0000-0002-0375-6300
FU Japan Society for the Promotion of Science [20244073]
FX We would like to express our appreciation to the engineers of
NEC/Toshiba Space Systems Ltd. (NTS), Nippon Antenna Co. Ltd., and Nippi
Corporation who developed the on-board instruments and the
sub-satellites. We would also like to thank the entire staff of the
SELENE project, especially the flight directors for both Rstar and Vstar
who supervised the tracking of these two sub-satellites. We would
especially like to thank all the colleagues at RISE Project, Mizusawa,
who helped with the VLBI observations and data correlation. We thank
Alex Konopliv (JPL) and two other anonymous reviewers for their comments
that helped to improve this paper. VLBI tracking data files and the new
model are available through the SELENE Data archive website at
http://www.soac.selene.isas.jaxa.jp/archive/. The models are also
available through the RISE Data archive website at
http://www.miz.nao.ac.jp/rise-pub/en. All figures were drawn using the
free software package GMT (Wessel and Smith 1991). Localised spherical
harmonic analyses were performed using the freely available software
archive SHTOOLS (available at http://www.ipgp.fr/similar to
wieczor/SHTOOLS/SHTOOLS.html). This work was supported by Grant-in-Aid
for Scientific Research (A) (No. 20244073) from the Japan Society for
the Promotion of Science. Finally, we like to mention that the gravity
experiments of SELENE would not have been possible without the expertise
of Fumio Fuke, an engineer of NTS, who sadly passed away 2 months after
the launch of the mission.
NR 53
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Z9 43
U1 0
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
EI 1432-1394
J9 J GEODESY
JI J. Geodesy
PD APR
PY 2011
VL 85
IS 4
BP 205
EP 228
DI 10.1007/s00190-010-0430-2
PG 24
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 748GI
UT WOS:000289377600002
ER
PT J
AU Waterbury, LD
Galindo, D
Villanueva, L
Nguyen, C
Patel, M
Borbridge, L
Attar, M
Schiffman, RM
Hollander, DA
AF Waterbury, L. David
Galindo, Danielle
Villanueva, Linda
Cathy Nguyen
Patel, Milan
Borbridge, Lisa
Attar, Mayssa
Schiffman, Rhett M.
Hollander, David A.
TI Ocular Penetration and Anti-inflammatory Activity of Ketorolac 0.45% and
Bromfenac 0.09% Against Lipopolysaccharide-Induced Inflammation
SO JOURNAL OF OCULAR PHARMACOLOGY AND THERAPEUTICS
LA English
DT Article
ID PROSTAGLANDIN E-2; CATARACT-SURGERY; VISCOUS VEHICLE; ANIMAL-MODELS;
TROMETHAMINE; 0.4-PERCENT; ABSORPTION; FORMULATIONS; INHIBITION;
EFFICACY
AB Purpose: Anti-inflammatory activity of topical nonsteroidal anti-inflammatory drugs is mediated by suppression of cyclooxygenase (COX) isoenzymes. This study compared ocular penetration and inflammation suppression of topical ketorolac 0.45% and bromfenac 0.09% ophthalmic solutions in a rabbit model.
Methods: At hour 0, 36 rabbits received ketorolac 0.45%, bromfenac 0.09%, or an artificial tear 3 times once every 20 min. Half of the rabbits in each group then received intravenous injections of lipopolysaccharide (LPS) and fluorescein isothiocyanate (FITC)-dextran at hour 1, and the other half at hour 10. Aqueous and iris-ciliary body (ICB) samples were collected in the former group at hour 2 (peak) and in the latter group at hour 11 (trough) An additional group of 6 animals received only FITC-dextran, and samples were collected 1 h later. Peak and trough nonsteroidal anti-inflammatory drug concentrations were compared with previously determined half-maximal inhibitory concentrations (IC(50)) for COX isoenzymes.
Results: Peak and trough aqueous and ICB concentrations of ketorolac were at least 7-fold or greater than those of bromfenac. At peak levels, both ketorolac 0.45% and bromfenac 0.09% significantly inhibited LPS-induced aqueous prostaglandin E(2) and FITC-dextran elevation (P < 0.01). At trough, both study drugs significantly inhibited LPS-induced aqueous prostaglandin E(2) elevation (P < 0.05), but only ketorolac 0.45% significantly reduced LPS-induced aqueous FITC-dextran elevation (P < 0.01). Aqueous and ICB ketorolac concentrations exceeded its IC(50) for COX-1 and COX-2 at peak and trough. Aqueous and ICB bromfenac levels exceeded its IC(50) for COX-2 at peak and trough, but not for COX-1 at trough aqueous levels and peak and trough ICB levels.
Conclusions: Both ketorolac 0.45% and bromfenac 0.09% effectively suppressed inflammation at peak. At trough, only ketorolac 0.45% effectively suppressed inflammation as measured by FITC-dextran leakage. The difference in inflammation suppression may be due to differences in tissue concentrations and/or greater COX-1 suppression by ketorolac 0.45%.
C1 [Waterbury, L. David] Raven Biosolut LLC, San Carlos, CA 94070 USA.
[Galindo, Danielle; Cathy Nguyen] NASA, Ames Res Ctr, Lifesource Biomed LLC, Moffett Field, CA 94035 USA.
[Villanueva, Linda; Patel, Milan; Borbridge, Lisa; Attar, Mayssa; Schiffman, Rhett M.; Hollander, David A.] Allergan Pharmaceut Inc, Irvine, CA 92715 USA.
RP Waterbury, LD (reprint author), Raven Biosolut LLC, POB 7001, San Carlos, CA 94070 USA.
EM david_waterbury@yahoo.com
FU Allergan, Inc., Irvine, CA; Allergan, Inc.
FX This study was funded by Allergan, Inc., Irvine, CA. L. David Waterbury
received research support from Allergan, Inc. D. Galindo and C. Nguyen
have no financial and/or conflicting interests to disclose. L.
Villanueva, M. Patel, L. Borbridge, M. Attar, R. M. Schiffman, and D. A.
Hollander are employees of Allergan, Inc.
NR 32
TC 6
Z9 6
U1 0
U2 0
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1080-7683
J9 J OCUL PHARMACOL TH
JI J. Ocular Pharmacol. Ther.
PD APR
PY 2011
VL 27
IS 2
BP 173
EP 178
DI 10.1089/jop.2010.0135
PG 6
WC Ophthalmology; Pharmacology & Pharmacy
SC Ophthalmology; Pharmacology & Pharmacy
GA 751NF
UT WOS:000289624100010
PM 21351868
ER
PT J
AU Hurwitz, MM
Newman, PA
Oman, LD
Molod, AM
AF Hurwitz, M. M.
Newman, P. A.
Oman, L. D.
Molod, A. M.
TI Response of the Antarctic Stratosphere to Two Types of El Nino Events
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID CHEMISTRY-CLIMATE MODELS; SEA-SURFACE TEMPERATURE; NORTHERN WINTER;
OSCILLATION; REANALYSIS; ENSEMBLE
AB This study is the first to identify a robust El Nino-Southern Oscillation (ENSO) signal in the Antarctic stratosphere. El Nino events between 1979 and 2009 are classified as either conventional "cold tongue" events (positive SST anomalies in the Nino-3 region) or "warm pool" events (positive SST anomalies in the Nino-4 region). The 40-yr ECMWF Re-Analysis (ERA-40), NCEP, and Modern Era Retrospective-Analysis for Research and Applications (MERRA) meteorological reanalyses are used to show that the Southern Hemisphere stratosphere responds differently to these two types of El Nino events. Consistent with previous studies, cold tongue events do not impact temperatures in the Antarctic stratosphere. During warm pool El Nino events, the poleward extension and increased strength of the South Pacific convergence zone favor an enhancement of planetary wave activity during September-November. On average, these conditions lead to higher polar stratospheric temperatures and a weakening of the Antarctic polar jet in November and December, as compared with neutral ENSO years. The phase of the quasi-biennial oscillation (QBO) modulates the stratospheric response to warm pool El Nino events; the strongest planetary wave driving events are coincident with the easterly phase of the QBO.
C1 [Hurwitz, M. M.] NASA, NASA Postdoctoral Program, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Molod, A. M.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
RP Hurwitz, MM (reprint author), NASA, NASA Postdoctoral Program, Goddard Space Flight Ctr, Code 613-3, Greenbelt, MD 20771 USA.
EM margaret.m.hurwitz@nasa.gov
RI Newman, Paul/D-6208-2012; Oman, Luke/C-2778-2009
OI Newman, Paul/0000-0003-1139-2508; Oman, Luke/0000-0002-5487-2598
FU NASA
FX MMH is supported by an appointment to the NASA Postdoctoral Program at
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. The authors thank NASA's MAP
program for funding.
NR 34
TC 18
Z9 18
U1 0
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD APR
PY 2011
VL 68
IS 4
BP 812
EP 822
DI 10.1175/2011JAS3606.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 749TC
UT WOS:000289491800010
ER
PT J
AU Azua-Bustos, A
Gonzalez-Silva, C
Mancilla, RA
Salas, L
Gomez-Silva, B
McKay, CP
Vicuna, R
AF Azua-Bustos, Armando
Gonzalez-Silva, Carlos
Mancilla, Rodrigo A.
Salas, Loreto
Gomez-Silva, Benito
McKay, Christopher P.
Vicuna, Rafael
TI Hypolithic Cyanobacteria Supported Mainly by Fog in the Coastal Range of
the Atacama Desert
SO MICROBIAL ECOLOGY
LA English
DT Article
ID 16S RIBOSOMAL-RNA; EXTRACELLULAR POLYSACCHARIDE; ENVIRONMENTAL
GRADIENTS; NORTHERN CHILE; HYPERARID CORE; SAND MULCHES; PCR PRIMERS;
CHINA HOT; WATER; COMMUNITY
AB The Atacama Desert is one of the driest places on Earth, with an arid core highly adverse to the development of hypolithic cyanobacteria. Previous work has shown that when rain levels fall below similar to 1 mm per year, colonization of suitable quartz stones falls to virtually zero. Here, we report that along the coast in these arid regions, complex associations of cyanobacteria, archaea, and heterotrophic bacteria inhabit the undersides of translucent quartz stones. Colonization rates in these areas, which receive virtually no rain but mainly fog, are significantly higher than those reported inland in the hyperarid zone at the same latitude. Here, hypolithic colonization rates can be up to 80%, with all quartz rocks over 20 g being colonized. This finding strongly suggests that hypolithic microbial communities thriving in the seaward face of the Coastal Range can survive with fog as the main regular source of moisture. A model is advanced where the development of the hypolithic communities under quartz stones relies on a positive feedback between fog availability and the higher thermal conductivity of the quartz rocks, which results in lower daytime temperatures at the quartz-soil interface microenvironment.
C1 [Azua-Bustos, Armando; Mancilla, Rodrigo A.; Salas, Loreto; Vicuna, Rafael] Pontificia Univ Catolica Chile, Fac Ciencias Biol, Dept Mol Genet & Microbiol, Santiago, Chile.
[Gonzalez-Silva, Carlos] Univ Arturo Prat, Ctr Invest Medio Ambiente CENIMA, Iquique, Chile.
[McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Azua-Bustos, Armando; Vicuna, Rafael] MIFAB, Santiago, Chile.
[Gomez-Silva, Benito] Univ Antofagasta, Fac Ciencias Salud, Dept Biomed, Antofagasta, Chile.
RP Azua-Bustos, A (reprint author), Pontificia Univ Catolica Chile, Fac Ciencias Biol, Dept Mol Genet & Microbiol, Alameda 340, Santiago, Chile.
EM ajazua@uc.cl
RI mancilla, rodrigo/C-8380-2011; azua-bustos, armando/P-8787-2016
FU Millennium Institute of Fundamental and Applied Biology, MIFAB (Chile)
FX This work was supported by the Millennium Institute of Fundamental and
Applied Biology, MIFAB (Chile). We also thank Alejandro Munizaga and
Ximena Verges for the technical support with microscopy methods.
NR 55
TC 33
Z9 33
U1 5
U2 30
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0095-3628
EI 1432-184X
J9 MICROB ECOL
JI Microb. Ecol.
PD APR
PY 2011
VL 61
IS 3
BP 568
EP 581
DI 10.1007/s00248-010-9784-5
PG 14
WC Ecology; Marine & Freshwater Biology; Microbiology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Microbiology
GA 747BK
UT WOS:000289295100009
PM 21188376
ER
PT J
AU Zhu, DH
Vaishampayan, PA
Venkateswaran, K
Fox, GE
AF Zhu, Dianhui
Vaishampayan, Parag A.
Venkateswaran, Kasthuri
Fox, George E.
TI STITCH: Algorithm to Splice, Trim, Identify, Track, and Capture the
Uniqueness of 16S rRNAs Sequence Pairs Using Public or In-house Database
SO MICROBIAL ECOLOGY
LA English
DT Article
ID FOR-BIOTECHNOLOGY-INFORMATION; POLYMERASE-CHAIN-REACTION; PCR;
AMPLIFICATION; IDENTIFICATION; FIDELITY; ARB; DNA; RESOURCES; BACTERIA
AB A comparison of variable regions within the 16S rRNA gene is widely used to characterize relationships between bacteria and to identify phylogenetic affiliation of unknown bacteria. In environmental studies, polymerase chain reaction amplification of 16S rRNA followed by cloning and sequencing of numerous individual clones is an extensively used molecular method for elucidating microbial diversity. The sequencing process typically utilizes a forward and reverse primer pair to produce two partial reads (similar to 700 to 800 base pairs each) that overlap and in total cover a large region of the full 16S rRNA sequence (similar to 1.5 k base). In a typical application, this approach rapidly generates very large numbers of 16S rRNA datasets that can overwhelm manual processing efforts leading to both delays and errors. In particular, the approach presents two computational challenges: (1) the assembly of a composite sequence from the two partial reads and (2) the subsequent appropriate identification of the organism represented by the newly sequenced clones. Herein, we describe a software package, search, trim, identify, track, and capture the uniqueness of 16S rRNAs using public and in-house database (STITCH), which offers automated sequence pair splicing and genetic identification, thus simplifying the computationally intensive analysis of large sequencing libraries. The STITCH software is freely accessible over the Internet at: http://prion.bchs.uh.edu/stitch/.
C1 [Vaishampayan, Parag A.; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
[Zhu, Dianhui; Fox, George E.] Univ Houston, Dept Biol & Biochem, Houston, TX 77204 USA.
RP Vaishampayan, PA (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, M-S 89-102,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM vaishamp@jpl.nasa.gov
NR 40
TC 2
Z9 2
U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0095-3628
EI 1432-184X
J9 MICROB ECOL
JI Microb. Ecol.
PD APR
PY 2011
VL 61
IS 3
BP 669
EP 675
DI 10.1007/s00248-010-9779-2
PG 7
WC Ecology; Marine & Freshwater Biology; Microbiology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Microbiology
GA 747BK
UT WOS:000289295100018
PM 21113709
ER
PT J
AU Shahzad, MMK
Mangala, LS
Han, HD
Lu, CH
Bottsford-Miller, J
Nishimura, M
Mora, EM
Lee, JW
Stone, RL
Pecot, CV
Thanapprapasr, D
Roh, JW
Gaur, P
Nair, MP
Park, YY
Sabnis, N
Deavers, MT
Lee, JS
Ellis, LM
Lopez-Berestein, G
McConathy, WJ
Prokai, L
Lacko, AG
Sood, AK
AF Shahzad, Mian M. K.
Mangala, Lingegowda S.
Han, Hee Dong
Lu, Chunhua
Bottsford-Miller, Justin
Nishimura, Masato
Mora, Edna M.
Lee, Jeong-Won
Stone, Rebecca L.
Pecot, Chad V.
Thanapprapasr, Duangmani
Roh, Ju-Won
Gaur, Puja
Nair, Maya P.
Park, Yun-Yong
Sabnis, Nirupama
Deavers, Michael T.
Lee, Ju-Seog
Ellis, Lee M.
Lopez-Berestein, Gabriel
McConathy, Walter J.
Prokai, Laszlo
Lacko, Andras G.
Sood, Anil K.
TI Targeted Delivery of Small Interfering RNA Using Reconstituted
High-Density Lipoprotein Nanoparticles
SO NEOPLASIA
LA English
DT Article
ID FOCAL ADHESION KINASE; ENDOTHELIAL GROWTH-FACTOR; OVARIAN-CARCINOMA;
SCAVENGER RECEPTOR; TUMOR ANGIOGENESIS; CANCER-CELLS; SR-BI;
CONSTITUTIVE ACTIVATION; ANTICANCER DRUGS; STAT3
AB RNA interference holds tremendous potential as a therapeutic approach, especially in the treatment of malignant tumors. However, efficient and biocompatible delivery methods are needed for systemic delivery of small interfering RNA (siRNA). To maintain a high level of growth, tumor cells scavenge high-density lipoprotein (HDL) particles by overexpressing its receptor: scavenger receptor type B1 (SR-B1). In this study, we exploited this cellular characteristic to achieve efficient siRNA delivery and established a novel formulation of siRNA by incorporating it into reconstituted HDL (rHDL) nanoparticles. Here, we demonstrate that rHDL nanoparticles facilitate highly efficient systemic delivery of siRNA in vivo, mediated by the SR-B1. Moreover, in therapeutic proof-of-concept studies, these nanoparticles were effective in silencing the expression of two proteins that are key to cancer growth and metastasis (signal transducer and activator of transcription 3 and focal adhesion kinase) in orthotopic mouse models of ovarian and colorectal cancer. These data indicate that an rHDL nanoparticle is a novel and highly efficient siRNA carrier, and therefore, this novel technology could serve as the foundation for new cancer therapeutic approaches.
C1 [Shahzad, Mian M. K.; Han, Hee Dong; Lu, Chunhua; Bottsford-Miller, Justin; Nishimura, Masato; Lee, Jeong-Won; Stone, Rebecca L.; Thanapprapasr, Duangmani; Roh, Ju-Won; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Dept Gynecol Oncol, Houston, TX 77030 USA.
[Shahzad, Mian M. K.] Univ Wisconsin, Dept Obstet & Gynecol, Div Gynecol Oncol, Sch Med & Publ Hlth, Madison, WI 53706 USA.
[Mangala, Lingegowda S.] Univ Space Res Assoc, Dept Radiat Biophys, NASA Johnson Space Ctr, Houston, TX USA.
[Mora, Edna M.; Gaur, Puja; Ellis, Lee M.] Univ Texas MD Anderson Canc Ctr, Dept Surg Oncol, Houston, TX 77030 USA.
[Mora, Edna M.] Univ Puerto Rico, Ctr Comprehens Canc, San Juan, PR 00936 USA.
[Mora, Edna M.] Univ Puerto Rico, Sch Med, San Juan, PR 00936 USA.
[Lee, Jeong-Won] Sungkyunkwan Univ, Sch Med, Samsung Med Ctr, Dept Obstet & Gynecol, Seoul, South Korea.
[Pecot, Chad V.] Univ Texas MD Anderson Canc Ctr, Dept Canc Med, Houston, TX 77030 USA.
[Nair, Maya P.; Sabnis, Nirupama; Prokai, Laszlo; Lacko, Andras G.] Univ N Texas, HSC, Dept Mol Biol & Immunol, Ft Worth, TX USA.
[Park, Yun-Yong; Lee, Ju-Seog] Univ Texas MD Anderson Canc Ctr, Dept Syst Biol, Houston, TX 77030 USA.
[Deavers, Michael T.] Univ Texas MD Anderson Canc Ctr, Dept Pathol, Houston, TX 77030 USA.
[Ellis, Lee M.; Lopez-Berestein, Gabriel; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Dept Canc Biol, Houston, TX 77030 USA.
[Lopez-Berestein, Gabriel] Univ Texas MD Anderson Canc Ctr, Dept Expt Therapeut, Houston, TX 77030 USA.
[Lopez-Berestein, Gabriel; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Ctr RNA Interference & Noncoding RNA, Houston, TX 77030 USA.
[McConathy, Walter J.] Texas Tech Univ, HSC, Dept Internal Med, Ft Worth, TX USA.
RP Sood, AK (reprint author), Univ Texas MD Anderson Canc Ctr, Dept Gynecol Oncol, 1155 Herman Pressler,Unit 1362, Houston, TX 77030 USA.
EM asood@mdanderson.org
RI lee, jw/O-6237-2014;
OI Prokai, Laszlo/0000-0002-4559-3458
FU GCF; National Institutes of Health [HD050128, CA109298, CA110793,
CA128797, RC2GM092599, U54 CA151668]; NCI [CA 101642, CA 009614];
Department of Defense [OC073399, OC093146, BC085265]; Ovarian Cancer
Research Fund, Inc; Zarrow Foundation; Marcus Foundation; University of
Texas MD Anderson Cancer Center SPORE in Ovarian Cancer [P50 CA083639];
Betty Ann Asche Murray Distinguished Professorship; Deborah Gonzalez
Women's Health Fellowship Award; Puerto Rico Comprehensive Cancer
Center; University of North Texas Health Science Center
FX This research was supported by the GCF Molly-Cade ovarian cancer
research grant, grants from the National Institutes of Health (Baylor
WRHR Scholarship grant: HD050128; CA109298, CA110793, CA128797,
RC2GM092599, U54 CA151668), NCI (T32 training grants CA 101642, CA
009614), Department of Defense (OC073399, OC093146, BC085265), a Program
Project Development Grant from the Ovarian Cancer Research Fund, Inc,
the Zarrow Foundation, The Marcus Foundation, the University of Texas MD
Anderson Cancer Center SPORE in Ovarian Cancer (P50 CA083639), the Betty
Ann Asche Murray Distinguished Professorship, Deborah Gonzalez Women's
Health Fellowship Award, the Puerto Rico Comprehensive Cancer Center,
Cowtown Cruisin' for the Cure, and a HER grant from the University of
North Texas Health Science Center.
NR 64
TC 82
Z9 89
U1 8
U2 51
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1476-5586
J9 NEOPLASIA
JI Neoplasia
PD APR
PY 2011
VL 13
IS 4
BP 309
EP U142
DI 10.1593/neo.101372
PG 17
WC Oncology
SC Oncology
GA 750FB
UT WOS:000289529400002
PM 21472135
ER
PT J
AU Halkides, D
Lee, T
Kida, S
AF Halkides, Daria
Lee, Tong
Kida, Shinichiro
TI Mechanisms controlling the seasonal mixed-layer temperature and salinity
of the Indonesian seas
SO OCEAN DYNAMICS
LA English
DT Article
DE Indonesian seas; Mixed layer; Seasonal heat budget; Seasonal salinity
budget; ECCO; Ocean-state estimation
ID MARITIME CONTINENT; CIRCULATION MODEL; UPPER OCEAN; PACIFIC;
THROUGHFLOW; PARAMETERIZATION; VARIABILITY; SENSITIVITY; REGION; GCM
AB We examine the seasonal mixed-layer temperature (MLT) and salinity (MLS) budgets in the Banda-Arafura Seas region (120-138A degrees E, 8-3A degrees S) using an ECCO ocean-state estimation product. MLT in these seas is relatively high during November-May (austral spring through fall) and relatively low during June-September (austral winter and the period associated with the Asian summer monsoon). Surface heat flux makes the largest contribution to the seasonal MLT tendency, with significant reinforcement by subsurface processes, especially turbulent vertical mixing. Temperature declines (the MLT tendency is negative) in May-August when seasonal insolation is smallest and local winds are strong due to the southeast monsoon, which causes surface heat loss and cooling by vertical processes. In particular, Ekman suction induced by local wind stress curl raises the thermocline in the Arafura Sea, bringing cooler subsurface water closer to the base of the mixed layer where it is subsequently incorporated into the mixed layer through turbulent vertical mixing; this has a cooling effect. The MLT budget also has a small, but non-negligible, semi-annual component since insolation increases and winds weaken during the spring and fall monsoon transitions near the equator. This causes warming via solar heating, reduced surface heat loss, and weakened turbulent mixing compared to austral winter and, to a lesser extent, compared to austral summer. Seasonal MLS is dominated by ocean processes rather than by local freshwater flux. The contributions by horizontal advection and subsurface processes have comparable magnitudes. The results suggest that ocean dynamics play a significant part in determining both seasonal MLT and MLS in the region, such that coupled model studies of the region should use a full ocean model rather than a slab ocean mixed-layer model.
C1 [Halkides, Daria] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90095 USA.
[Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kida, Shinichiro] Japan Agcy Marine Earth Sci & Technol, Earth Simulator Ctr, Yokohama, Kanagawa, Japan.
RP Halkides, D (reprint author), Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90095 USA.
EM halkides@jpl.nasa.gov
RI Kida, Shinichiro/E-9137-2014
OI Kida, Shinichiro/0000-0002-9471-4316
FU NASA; PO.DAAC; KAKENHI [21840066]
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. Support by
PO.DAAC (http://podaac.jpl.nasa.gov) is acknowledged. S. Kida was
supported by KAKENHI (21840066).
NR 40
TC 6
Z9 6
U1 0
U2 11
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1616-7341
EI 1616-7228
J9 OCEAN DYNAM
JI Ocean Dyn.
PD APR
PY 2011
VL 61
IS 4
BP 481
EP 495
DI 10.1007/s10236-010-0374-3
PG 15
WC Oceanography
SC Oceanography
GA 750ES
UT WOS:000289528400007
ER
PT J
AU Kwok, R
Untersteiner, N
AF Kwok, Ronald
Untersteiner, Norbert
TI The thinning of Arctic sea ice
SO PHYSICS TODAY
LA English
DT Article
ID MODEL
C1 [Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Untersteiner, Norbert] Univ Washington, Seattle, WA 98195 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
NR 14
TC 66
Z9 69
U1 1
U2 23
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0031-9228
EI 1945-0699
J9 PHYS TODAY
JI Phys. Today
PD APR
PY 2011
VL 64
IS 4
BP 36
EP 41
PG 6
WC Physics, Multidisciplinary
SC Physics
GA 748NS
UT WOS:000289397900015
ER
PT J
AU Gopalswamy, N
AF Gopalswamy, Nat
TI Mukul Ranjan Kundu obituary
SO PHYSICS TODAY
LA English
DT Biographical-Item
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Gopalswamy, Nat/D-3659-2012;
OI Gopalswamy, Nat/0000-0001-5894-9954
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0031-9228
EI 1945-0699
J9 PHYS TODAY
JI Phys. Today
PD APR
PY 2011
VL 64
IS 4
BP 71
EP 71
PG 1
WC Physics, Multidisciplinary
SC Physics
GA 748NS
UT WOS:000289397900019
ER
PT J
AU Jimenez-Escalona, JC
Granados, HD
Realmuto, VJ
AF Carlos Jimenez-Escalona, Jose
Delgado Granados, Hugo
Realmuto, Vincent J.
TI Use of MODIS images to study eruptive clouds from Volcan de Fuego de
Colima (Mexico) and applications on volcano monitoring
SO GEOFISICA INTERNACIONAL
LA English
DT Article
DE remote sensing; volcanic emission; MODIS; satellite image; Colima
volcano; volcanic cloud
ID ASH CLOUDS; DE-COLIMA; EMISSIONS
AB Volcano monitoring using satellite images may provide periodic information on gas emission fluctuations such as SO(2) emissions related to the processes occurring inside volcanoes. This study analyses a period of 36 days (May 10 to June 15, 2005) of processing 113 MODIS images for the detection of SO(2). Within this period it was also possible to detect and quantify 8 of 15 explosive events reported by the Washington VAAC. With the satellite images as tools for monitoring the volcanic emissions, it was possible to determine three cases related to volcanic ashes: 1) follow up of volcanic ash and gases transported by wind, 2) calculation of ash-cloud residence time in the atmosphere, 3) effects of shearing winds during the ascent of an ash plume.
Regarding the continuous monitoring of passive emissions of SO(2), there is a relationship among explosive events and increasing peaks of SO(2) emission suggesting a difference of approximately 2 days between the two events that may anticipate the type of behavior of the volcano.
C1 [Carlos Jimenez-Escalona, Jose; Delgado Granados, Hugo] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico.
[Carlos Jimenez-Escalona, Jose] Inst Politecn Nacl, ESIME U Ticoman, Mexico City 07340, DF, Mexico.
[Realmuto, Vincent J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jimenez-Escalona, JC (reprint author), Univ Nacl Autonoma Mexico, Inst Geofis, Ciudad Univ, Mexico City 04510, DF, Mexico.
EM jjimeneze@ipn.mx
RI Delgado Granados, Hugo/J-3056-2013;
OI Delgado Granados, Hugo/0000-0001-5263-7968; Jimenez_Escalona, Jose
Carlos/0000-0001-9309-5245
FU EHaz program
FX The first author is grateful to William I. Rose for his assistance while
in Michigan Tech for learning remote sensing methods, This research was
partially funded by the EHaz program.
NR 29
TC 2
Z9 2
U1 1
U2 4
PU INST GEOPHYSICS UNAM
PI MEXICO
PA APDO POSTAL 22-118, DEL TLALPAN, MEXICO, 14000 D F, MEXICO
SN 0016-7169
J9 GEOFIS INT
JI Geofis. Int.
PD APR-JUN
PY 2011
VL 50
IS 2
BP 199
EP 210
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 746BU
UT WOS:000289217400006
ER
PT J
AU Zahnle, K
Freedman, RS
Catling, DC
AF Zahnle, Kevin
Freedman, Richard S.
Catling, David C.
TI Is there methane on Mars?
SO ICARUS
LA English
DT Article
DE Atmospheres, Chemistry; Mars, Atmosphere; Spectroscopy; Photochemistry
ID MARTIAN DUST DEVILS; ATMOSPHERIC CHEMISTRY; NOBLE-GASES; OXIDANT
ENHANCEMENT; PHOTOCHEMICAL DATA; CARBON-MONOXIDE; H2O PHOTOLYSIS;
ISOTOPIC CO2; ORIGIN; LIFE
AB There have been several reports of methane on Mars at the 10-60 ppbv level. Most suggest that methane is both seasonally and latitudinally variable. Here we review why variable methane on Mars is physically and chemically implausible, and then we critically review the published reports. There is no known mechanism for destroying methane chemically on Mars. But if there is one, methane oxidation would deplete the O-2 in Mars's atmosphere in less than 10,000 years unless balanced by an equally large unknown source of oxidizing power. Physical sequestration does not raise these questions, but adsorption in the regolith or condensation in clathrates ignore competition for adsorption sites or are inconsistent with clathrate stability, respectively. Furthermore, any mechanism that relies on methane's van der Waals' attraction is inconsistent with the continued presence of Xe in the atmosphere at the 60 ppbv level. We then use the HITRAN database and transmission calculations to identify and characterize the absorption lines that would be present on Earth or Mars at the wavelengths of the published observations. These reveal strong competing telluric absorption that is most problematic at just those wavelengths where methane's signature seems most clearly seen from Earth. The competing telluric lines must be removed with models. The best case for martian methane was made for the (CH4)-C-12 nu(3) R0 and R1 lines seen in blueshift when Mars was approaching Earth in early 2003 (Mumma, M.J., Villanueva, G.L., Novak, RE., Hewagama, T., Bonev, B.P., DiSanti, MA., Mandell, A.M., Smith, M.D. [2009]. Science 323, 1041-1045). For these the Doppler shift moves the two martian lines into near coincidence with telluric (CH4)-C-13 nu(3) R1 and R2 lines that are 10-50x stronger than the inferred martian lines. By contrast, the (CH4)-C-12 nu(3) R0 and R1 lines when observed in redshift do not contend with telluric (CH4)-C-13. For these lines, Mumma et al.'s observations and analyses are consistent with an upper limit on the order of 3 ppbv. Published by Elsevier Inc.
C1 [Zahnle, Kevin; Freedman, Richard S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Catling, David C.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
RP Zahnle, K (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
EM Kevin.J.Zahnle@NASA.gov
RI Catling, David/D-2082-2009;
OI Catling, David/0000-0001-5646-120X
FU NASA
FX We thank Todd Clancy, Francois Forget, Colin Goldblatt, Tom Greene,
Robert Haberle, Jim Lyons, Chris McKay, and Victoria Meadows for helpful
comments, comprehensive discussions, several corrections, and key
insights. We especially thank Michael Mumma and Geronimo Villanueva for
their openness and the considerable help and encouragement they have
given us in all aspects of this work. We also thank Paul Wennberg, Mike
Mumma and an anonymous reviewer for careful reviews correcting and
improving the manuscript. This work was supported by NASA's Exobiology
Program.
NR 61
TC 72
Z9 75
U1 5
U2 35
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2011
VL 212
IS 2
BP 493
EP 503
DI 10.1016/j.icarus.2010.11.027
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745PM
UT WOS:000289178100005
ER
PT J
AU Davila, AF
Gross, C
Marzo, GA
Fairen, AG
Kneissl, T
McKay, CP
Dohm, JM
AF Davila, Alfonso F.
Gross, Christoph
Marzo, Giuseppe A.
Fairen, Alberto G.
Kneissl, Thomas
McKay, Christopher P.
Dohm, James M.
TI A large sedimentary basin in the Terra Sirenum region of the southern
highlands of Mars
SO ICARUS
LA English
DT Article
DE Evaporites; Basin; Highlands; Noachian; Water
ID ATACAMA DESERT; AQUEOUS ENVIRONMENTS; IMPACT CRATERS; EVAPORITES; CHILE;
PHYLLOSILICATES; EVOLUTION; MINERALS; CLIMATE; MISSION
AB Different lines of evidence point to hydrological cycling in the martian past. The extent, duration, and magnitude of this cycling remains unclear, as well as the magnitude of aqueous processes on the surface. Here, we provide geomorphic and mineralogic evidence of a large inter-crater sedimentary basin located in the Terra Sirenum region, which was once covered by a body of liquid water with an areal extent of at least 30,000 km(2) and a depth of approximately 200 m. The topographic basin, which is modified by a number of large impact craters, is partly controlled by ancient impact and tectonic structures. As a result of evaporation of the large body of water, salt flats formed in the lowest topographic reaches of the basin. Hydrated phyllosilicates occur in close proximity to the salt flats and in the ejecta and rim materials of small impact craters with stratigraphic relations that suggest that they underlie the evaporite deposits. Crater statistics place the maximum age of aqueous activity during the Late Noachian epoch. The relatively pristine mineral deposits in the basin have a high potential to yield information of the geochemistry and water activity during the ancient Noachian Period when conditions were seemingly more conducive to life. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Davila, Alfonso F.; Marzo, Giuseppe A.; Fairen, Alberto G.; McKay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Davila, Alfonso F.; Fairen, Alberto G.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA.
[Gross, Christoph; Kneissl, Thomas] Free Univ Berlin, Inst Geol Sci Planetary Sci & Remote Sensing, D-12249 Berlin, Germany.
[Marzo, Giuseppe A.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Dohm, James M.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85719 USA.
RP Davila, AF (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM adavila@seti.org
RI Davila, Alfonso/A-2198-2013; Dohm, James/A-3831-2014; Marzo,
Giuseppe/A-9765-2015
OI Davila, Alfonso/0000-0002-0977-9909;
FU Helmholtz Association through the research alliance "Planetary Evolution
and Life"
FX We wish to thank the comments and suggestions of two anonymous
reviewers, which greatly improved the manuscript. Research by C.G. and
T.K. was supported by the Helmholtz Association through the research
alliance "Planetary Evolution and Life".
NR 56
TC 10
Z9 10
U1 1
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2011
VL 212
IS 2
BP 579
EP 589
DI 10.1016/j.icarus.2010.12.023
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745PM
UT WOS:000289178100011
ER
PT J
AU Busch, MW
Ostro, SJ
Benner, LAM
Brozovic, M
Giorgini, JD
Jao, JS
Scheeres, DJ
Magri, C
Nolan, MC
Howell, ES
Taylor, PA
Margot, JL
Brisken, W
AF Busch, Michael W.
Ostro, Steven J.
Benner, Lance A. M.
Brozovic, Marina
Giorgini, Jon D.
Jao, Joseph S.
Scheeres, Daniel J.
Magri, Christopher
Nolan, Michael C.
Howell, Ellen S.
Taylor, Patrick A.
Margot, Jean-Luc
Brisken, Walter
TI Radar observations and the shape of near-Earth ASTEROID 2008 EV5
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids, Surfaces; Asteroids, Dynamics; Radar observations
ID BINARY ASTEROIDS; 2867 STEINS; 1999 KW4; YORP; POPULATION; YARKOVSKY;
REGOLITH; HAYABUSA; SPINS
AB We observed the near-Earth ASTEROID 2008 EV5 with the Arecibo and Goldstone planetary radars and the Very Long Baseline Array during December 2008. EV5 rotates retrograde and its overall shape is a 400 +/- 50 m oblate spheroid. The most prominent surface feature is a ridge parallel to the asteroid's equator that is broken by a concavity about 150 m in diameter. Otherwise the asteroid's surface is notably smooth on decameter scales. EV5's radar and optical albedos are consistent with either rocky or stony-iron composition. The equatorial ridge is similar to structure seen on the rubble-pile near-Earth asteroid (66391) 1999 KW4 and is consistent with YORP spin-up reconfiguring the asteroid in the past. We interpret the concavity as an impact crater. Shaking during the impact and later regolith redistribution may have erased smaller features, explaining the general lack of decameter-scale surface structure. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Busch, Michael W.; Margot, Jean-Luc] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Ostro, Steven J.; Benner, Lance A. M.; Brozovic, Marina; Giorgini, Jon D.; Jao, Joseph S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Scheeres, Daniel J.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Magri, Christopher] Univ Maine, Farmington, ME 04938 USA.
[Nolan, Michael C.; Howell, Ellen S.; Taylor, Patrick A.] Arecibo Observ, Arecibo, PR 00612 USA.
[Margot, Jean-Luc] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Brisken, Walter] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Busch, MW (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, 595 Charles Young Dr E, Los Angeles, CA 90095 USA.
EM mbusch@ess.ucla.edu
RI Margot, Jean-Luc/A-6154-2012; Nolan, Michael/H-4980-2012
OI Margot, Jean-Luc/0000-0001-9798-1797; Nolan, Michael/0000-0001-8316-0680
FU National Science Foundation; National Aeronautics and Space
Administration (NASA); Hertz Foundation
FX The Goldstone Solar System Radar, Arecibo Observatory, and NRAO Socorro
8: Green Bank staff helped to obtain the data presented here. We thank
A. Galad, B.W. Koehn, M.D. Hicks, and V. Reddy for providing EV5's
rotation period and spectral type from their optical and infrared
observations in advance of publication. The Arecibo Observatory is part
of the National Astronomy and Ionosphere Center, which is operated by
Cornell University under a cooperative agreement with the National
Science Foundation. The NRAO is run by Associated Universities, Inc. for
the National Science Foundation. Some of this work was performed at the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration (NASA).
This paper is based in part on work funded by NASA under the Science
Mission Directorate Research and Analysis Programs. M.W. Busch was
supported by the Hertz Foundation. Our observations of EV5 are dedicated
to the memory of Steven Ostro.
NR 46
TC 25
Z9 26
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 APR
PY 2011
VL 212
IS 2
BP 649
EP 660
DI 10.1016/j.icarus.2011.01.013
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745PM
UT WOS:000289178100017
ER
PT J
AU Hendrix, AR
Cassidy, TA
Johnson, RE
Paranicas, C
Carlson, RW
AF Hendrix, Amanda R.
Cassidy, Timothy A.
Johnson, Robert E.
Paranicas, Chris
Carlson, Robert W.
TI Europa's disk-resolved ultraviolet spectra: Relationships with plasma
flux and surface terrains
SO ICARUS
LA English
DT Article
DE Europa; Ices, UV spectroscopy; Jupiter, Satellites; Ultraviolet
observations; Satellites, Composition
ID ICY GALILEAN SATELLITES; MAGNETOSPHERIC ION-BOMBARDMENT; SULFURIC-ACID;
WATER ICE; PHOTOMETRY; SPECTROMETER; IMPLANTATION; RADIOLYSIS; HYDRATE;
ALBEDO
AB The full set of high-resolution observations from the Galileo Ultraviolet Spectrometer (UVS) is analyzed to look for spectral trends across the surface of Europa. We provide the first disk-resolved map of the 280 nm SO(2) absorption feature and investigate its relationship with sulfur and electron flux distributions as well as with surface features and relative surface ages. Our results have implications for exogenic and endogenic sources. The large-scale pattern in SO(2) absorption band depth is again shown to be similar to the pattern of sulfur ion implantation, but with strong variations in band depth based on terrain. In particular, the young chaos units show stronger SO(2) absorption bands than expected from the average pattern of sulfur ion flux, suggesting a local source of SO(2) in those regions, or diapiric heating that leads to a sulfur-rich lag deposit.
While the SO(2) absorption feature is confined to the trailing hemisphere, the near UV albedo (300-310 nm) has a global pattern with a minimum at the center of the trailing hemisphere and a maximum at the center of the leading hemisphere. The global nature of the albedo pattern is suggestive of an exogenic source, and several possibilities are discussed. Like the SO(2) absorption, the near UV albedo also has local variations that depend on terrain type and age. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Hendrix, Amanda R.; Cassidy, Timothy A.; Carlson, Robert W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Johnson, Robert E.] Univ Virginia, Charlottesville, VA 22904 USA.
[Paranicas, Chris] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Hendrix, AR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM arh@jpl.nasa.gov
RI Paranicas, Christopher/B-1470-2016
OI Paranicas, Christopher/0000-0002-4391-8255
FU Jupiter System Data Analysis Program; Planetary Geology and Geophysics
Program; National Aeronautics and Space Administration
FX This paper has benefited from good conversations with John Cooper, Gary
Hansen, Karl Hibbitts and Bob Nelson, Karen Simmons and Charles Barth.
Charles Hord was the PI of the Galileo UVS. This work was supported by
the Jupiter System Data Analysis Program and the Planetary Geology and
Geophysics Program. 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.
NR 46
TC 14
Z9 14
U1 0
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2011
VL 212
IS 2
BP 736
EP 743
DI 10.1016/j.icarus.2011.01.023
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745PM
UT WOS:000289178100025
ER
PT J
AU Williams, DA
Radebaugh, J
Lopes, RMC
Stofan, E
AF Williams, David A.
Radebaugh, Jani
Lopes, Rosaly M. C.
Stofan, Ellen
TI Geomorphologic mapping of the Menrva region of Titan using Cassini RADAR
data
SO ICARUS
LA English
DT Article
DE Radar observations; Geological processes
ID DIELECTRIC-PROPERTIES; RADIOMETRY DATA; ICY SATELLITES; SURFACE; MAPPER;
SAR; DIVERSITY; DUNES
AB We made a detailed geomorphologic map of the Menrva region of Titan, using Cassini RADAR data as our map base. Using similar techniques and approaches that were applied to mapping Magellan radar images of Venus, and earlier, more generalized Titan maps, we were able to define and characterize 10 radar morphologic units, along with inferred dunes and fluvial channels, from the RADAR data. Structural features, such as scarps, ridges, and lineaments were also identified. Using principles of superposition, cross-cutting, and embayment relations we created a sequence of map units for this region. We interpret Menrva to be a 440 km wide degraded impact basin, in agreement with earlier studies by Elachi et al. (Elachi, C. et al. [2006]. Nature 441, 709-713) and Wood et al. (Wood, C.A., Lorenz, R., Kirk, R., Lopes, R., Mitchell, K., Stofan, E., and the Cassini RADAR Team [2010]. Icarus 206, 334-344), and identify it as the oldest feature in the map region. Exogenic processes including hydrocarbon fluid channelization forming the Elivagar Flumina channel network and dune fields resulting from aeolian activity are the current geologic processes dominating our map area, and these processes have contributed to the erosion of the crater's ejecta field. There is evidence of multiple episodes of channel formation, erosion and burial by aeolian deposits, as observed elsewhere on Titan by e.g., Barnes et al. (Barnes, J.W. et al. [2005]. Icarus 195,400-414). Channel outflow regions have morphologies suggestive of streams formed by flash floods, and dune fields are small and restricted rather than forming large dune seas, consistent with a desert-like environment for this region with low supply of hydrocarbon particles, also consistent with other studies by e.g.. Lorenz et al. (Lorenz, R.D. et al. [2008a]. Planet. Space Sci. 56, 1132-1144). There is no evidence of cryovolcanism or non-impact-related tectonic activity in the Menrva region, although this region is too small to infer anything about the roles of these processes elsewhere on Titan. This work suggests detailed geomorphologic mapping can confidently be applied to Cassini RADAR data, and we suggest that more extensive mapping should be done using RADAR, ISS, and VIMS data geographically distributed across Titan to assess its usefulness for a future combined RADAR-ISS-VIMS-based global geologic map. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Radebaugh, Jani] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
[Lopes, Rosaly M. C.] CALTECH, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA.
[Stofan, Ellen] Proxemy Res Inc, Rectortown, VA 20140 USA.
RP Williams, DA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM david.williams@asu.edu
RI Lopes, Rosaly/D-1608-2016
OI Lopes, Rosaly/0000-0002-7928-3167
NR 50
TC 8
Z9 8
U1 1
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2011
VL 212
IS 2
BP 744
EP 750
DI 10.1016/j.icarus.2011.01.014
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745PM
UT WOS:000289178100026
ER
PT J
AU Anderson, CM
Samuelson, RE
AF Anderson, Carrie M.
Samuelson, Robert E.
TI Titan's aerosol and stratospheric ice opacities between 18 and 500 mu m:
Vertical and spectral characteristics from Cassini CIRS
SO ICARUS
LA English
DT Article
DE Titan; Radiative transfer; Ices
ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; COMPOSITE INFRARED SPECTROMETER;
SPECTROSCOPIC DATABASE; CONDENSATE CLOUDS; THERMAL EMISSION;
UPPER-ATMOSPHERE; JOVIAN PLANETS; PAIRS; TEMPERATURES; MODEL
AB Vertical distributions and spectral characteristics of Titan's photochemical aerosol and stratospheric ices are determined between 20 and 560 cm(-1) (500-18 mu m) from the Cassini Composite Infrared Spectrometer (CIRS). Results are obtained for latitudes of 15 degrees N, 15 degrees S, and 58 degrees S. where accurate temperature profiles can be independently determined.
In addition, estimates of aerosol and ice abundances at 62 degrees N relative to those at 15 degrees S are derived. Aerosol abundances are comparable at the two latitudes, but stratospheric ices are similar to 3 times more abundant at 62 degrees N than at 15 degrees S. Generally, nitrile ice clouds (probably HCN and HC3N), as inferred from a composite emission feature at similar to 160 cm(-1), appear to be located over a narrow altitude range in the stratosphere centered at similar to 90 km. Although most abundant at high northern latitudes, these nitrile ice clouds extend down through low latitudes and into mid southern latitudes, at least as far as 58 degrees S.
There is some evidence of a second ice cloud layer at similar to 60 km altitude at 58 degrees S associated with an emission feature at similar to 80 cm(-1). We speculate that the identify of this cloud may be due to C2H6 ice, which in the vapor phase is the most abundant hydrocarbon (next to CH4) in the stratosphere of Titan.
Unlike the highly restricted range of altitudes (50-100 km) associated with organic condensate clouds, Titan's photochemical aerosol appears to be well-mixed from the surface to the top of the stratosphere near an altitude of 300 km, and the spectral shape does not appear to change between 15 degrees N and 58 degrees S latitude. The ratio of aerosol-to-gas scale heights range from 1.3-2.4 at about 160 km to 1.1-1.4 at 300 km, although there is considerable variability with latitude. The aerosol exhibits a very broad emission feature peaking at similar to 140 cm-1. Due to its extreme breadth and low wavenumber, we speculate that this feature may be caused by low-energy vibrations of two-dimensional lattice structures of large molecules. Examples of such molecules include polycyclic aromatic hydrocarbons (PAHs) and nitrogenated aromatics.
Finally, volume extinction coefficients N chi(E) derived from 15 degrees S CIRS data at a wavelength of lambda = 62.5 mu m are compared with those derived from the 10 degrees S Huygens Descent Imager/Spectral Radiometer (DISR) data at 1.583 mu m. This comparison yields volume extinction coefficient ratios N chi(E)(1.583 mu m)/N chi(E)(62.5 mu m) of roughly 70 and 20, respectively, for Titan's aerosol and stratospheric ices. The inferred particle cross-section ratios chi(E)(1.583 mu m)/chi(E)(62.5 mu m) appear to be consistent with sub-micron size aerosol particles, and effective radii of only a few microns for stratospheric ice cloud particles. Published by Elsevier Inc.
C1 [Anderson, Carrie M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Samuelson, Robert E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Anderson, CM (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM carrie.m.anderson@nasa.gov
RI Anderson, Carrie/C-8097-2012
FU Cassini project; NASA; NSF
FX We would like to extend our thanks to Lyn Doose for providing the
tabulated Huygens DISR aerosol volume extinction coefficients at 1.583
mu m. We also thank Marla Moore for providing laboratory absorption
coefficients for HCN and HC3N ice mixtures. Thanks to Richard
Achterberg for providing CIRS Titan temperature structures. C.M.A. was
supported in part by the Cassini project and the NASA Cassini Data
Analysis Program. R.E.S. was supported in part by the Cassini project
and the NSF Planetary Astronomy Program.
NR 62
TC 44
Z9 45
U1 2
U2 19
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2011
VL 212
IS 2
BP 762
EP 778
DI 10.1016/j.icarus.2011.01.024
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745PM
UT WOS:000289178100028
ER
PT J
AU Moore, JM
Pappalardo, RT
AF Moore, Jeffrey M.
Pappalardo, Robert T.
TI Titan: An exogenic world?
SO ICARUS
LA English
DT Article
DE Saturn, satellites; Titan; Titan, atmosphere; Titan, hydrology; Titan,
surface
ID HUYGENS LANDING SITE; CASSINI RADAR OBSERVATIONS; SATURNS MOON TITAN;
GALILEAN SATELLITES; INTERNAL STRUCTURE; MERCURIAN VOLCANISM;
AMMONIUM-SULFATE; ICY SATELLITES; DARK TERRAIN; EARLY MARS
AB All landforms on Titan that are unambiguously identifiable can be explained by exogenic processes (aeolian, fluvial, impact cratering, and mass wasting). Previous suggestions of endogenically produced cryovolcanic constructs and flows have, without exception, lacked conclusive diagnostic evidence. The modification of sparse recognizable impact craters (themselves exogenic) can be explained by aeolian and fluvial erosion. Tectonic activity could be driven by global thermal evolution or external forcing, rather than by active interior processes. A lack of cryovolcanism would be consistent with geophysical inferences of a relatively quiescent interior: incomplete differentiation, only minor tidal heating, and possibly a lack of internal convection today. Titan might be most akin to Callisto with weather: an endogenically relatively inactive world with a cool interior. We do not aim to disprove the existence of any and all endogenic activity at Titan, nor to provide definitive alternative hypotheses for all landforms, but instead to inject a necessary level of caution into the discussion. The hypothesis of Titan as a predominantly exogenic world can be tested through additional Cassini observations and analyses of putative cryovolcanic features, geophysical and thermal modeling of Titan's interior evolution, modeling of icy satellite landscape evolution that is shaped by exogenic processes alone, and consideration of possible means for supplying Titan's atmospheric constituents that do not rely on cryovolcanism. Published by Elsevier Inc.
C1 [Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Moore, JM (reprint author), NASA, Ames Res Ctr, Div Space Sci, M-S 245-3, Moffett Field, CA 94035 USA.
EM jeff.moore@nasa.gov; robert.pappalardo@jpl.nasa.gov
FU Outer Planets Research Program; Cassini Project; National Aeronautics
and Space Administration
FX We thank Amy Barr, Bruce Bills, Geoff Collins, Ken Edgett, Alan Howard,
Krishan Khurana, Randy Kirk, Bill McKinnon, Giuseppe Mitri, Francis
Nimmo, Conor Nixon, Flora Paganelli, Paul Schenk, Larry Soderblom,
Christophe Sotin, Don Wilhelms, and Kevin Zahnle for valuable reviews
and discussions on various aspects of this research. We are especially
grateful for the formal reviews of Jani Radebaugh, Ellen Stofan, and an
anonymous reviewer collectively whose comments substantially improved
this report. We acknowledge Snowpacalypse 2010 for making the
long-awaited completion of this paper possible. Funding for this work
was provided by an Outer Planets Research Program grant (JMM) and the
Cassini Project (RTP). The portion of this work performed by RTP was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 159
TC 37
Z9 37
U1 3
U2 30
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 APR
PY 2011
VL 212
IS 2
BP 790
EP 806
DI 10.1016/j.icarus.2011.01.019
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745PM
UT WOS:000289178100030
ER
PT J
AU Buratti, BJ
Bauer, JM
Hicks, MD
Hillier, JK
Verbiscer, A
Hammel, H
Schmidt, B
Cobb, B
Herbert, B
Garsky, M
Ward, J
Foust, J
AF Buratti, B. J.
Bauer, J. M.
Hicks, M. D.
Hillier, J. K.
Verbiscer, A.
Hammel, H.
Schmidt, B.
Cobb, B.
Herbert, B.
Garsky, M.
Ward, J.
Foust, J.
TI Photometry of Triton 1992-2004: Surface volatile transport and discovery
of a remarkable opposition surge
SO ICARUS
LA English
DT Article
DE Triton; Satellites, Surfaces; Satellites, Atmospheres
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DISK-INTEGRATED PHOTOMETRY;
OUTER PLANET SATELLITES; HUBBLE-SPACE-TELESCOPE; COHERENT BACKSCATTER;
URANIAN SATELLITES; RADIATIVE-TRANSFER; LIGHT-CURVE; VARIABILITY;
BRIGHTNESS
AB Triton, the large satellite of Neptune, was imaged by the Voyager 2 spacecraft in 1989 with dark plumes originating in its volatile-rich south polar region. Southern summer solstice, a time when seasonal volatile transport should be at a maximum, occurred in 2001. Ground-based observations of Triton's rotational light curve obtained from Table Mountain Observatory in 2000-2004 reveal volatile transport on its surface. When compared with a static frost model constructed from Voyager images, the light curve shows an increase in total amplitude. An earlier light curve obtained in 1992 from Mauna Kea Observatory is consistent with the static frost model. This movement of volatiles on the surface agrees with recent imaging results from the Hubble Space Telescope (Bauer, J.M., Buratti, B.J., Li, J.-Y., Mosher, J.A., Hicks, M.D., Schmidt, BE., Goguen, J.D. [2010]. Astrophys. J. 723, L49-L52). The changes in the light curve can be explained by the transport of nitrogen frost on the surface or by the uncovering of bedrock of less volatile methane. We also find that Triton exhibits a large opposition surge at solar phase angles less than 0.1 degrees. This surge cannot be entirely explained by the effects of coherent backscatter. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Buratti, B. J.; Bauer, J. M.; Hicks, M. D.; Schmidt, B.; Cobb, B.; Herbert, B.; Garsky, M.; Ward, J.; Foust, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hillier, J. K.] Grays Harbor Coll, Aberdeen, WA 98520 USA.
[Verbiscer, A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Hammel, H.] Space Sci Inst, Boulder, CO 80301 USA.
RP Buratti, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Bonnie.Buratti@jpl.nasa.gov
OI Schmidt, Britney/0000-0001-7376-8510
FU National Aeronautics and Space Administration; Planetary Geology and
Geophysics Undergraduate Research Program
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology under contract to the National
Aeronautics and Space Administration. We thank NASA's Planetary
Astronomy and Planetary Geology and Geophysics Programs for support. The
students were sponsored by NASA's Undergraduate Student Research
Program, New York Space Grant, and the Planetary Geology and Geophysics
Undergraduate Research Program. Copyright 2010 all rights reserved.
NR 59
TC 9
Z9 9
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 APR
PY 2011
VL 212
IS 2
BP 835
EP 846
DI 10.1016/j.icarus.2011.01.012
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745PM
UT WOS:000289178100033
ER
PT J
AU Firoz, KA
Moon, YJ
Cho, KS
Hwang, J
Park, YD
Kudela, K
Dorman, LI
AF Firoz, K. A.
Moon, Y. -J.
Cho, K. -S.
Hwang, J.
Park, Y. D.
Kudela, K.
Dorman, L. I.
TI On the relationship between ground level enhancement and solar flare
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID X-RAY FLARES; PROTON EVENTS; ENERGETIC PARTICLES; NEUTRON-MONITORS;
UPPER LIMIT; INDEX; TIMES; SOLAR-CYCLE-23; EMISSION; CYCLES
AB We made an effort to understand the associations and relationships between ground level enhancement (GLE) events and solar flares for the time period of 1986-2006. Our results show that, on average, the GLE event-associated solar flare (similar to 0.2 x 10(-4) W/m(2)) is much stronger than the non-GLE-associated solar flare (similar to 0.3 x 10(-5) W/m(2)). The findings have also been supported by the solar flare indices that, on average, the GLE event-associated solar flare index (similar to 35.01) is much higher than the non-GLE-associated solar flare index (similar to 4.88). However, this association does not seem to precisely imply that GLEs can occur because of a solar flare, so we examined cross correlations between GLE events and simultaneous solar flares. We found that most (similar to 78%) of the highest correlations (r > 0.8) took place during an X class flare. There is no clear indication that the more the time lag, the less or more is the correlation or vice versa. Overall, 50% of the high correlations took place at higher time lag (>= 65 min), and similar to 36% of the high correlations took place at lower time lag (<= 40 min), while the rest (similar to 14%) of the correlations were abruptly high and low at medium time lag (> 40 and < 65 min). On the basis of the results of cross correlations, we suggest that the intensive portions of solar flares should be responsible for causing GLEs and that the direct proportionality of the time-integrated intensive portion of a flare with the impulsive phase of a GLE event seems to be the main property for comprehending the mechanism.
C1 [Firoz, K. A.; Cho, K. -S.; Hwang, J.; Park, Y. D.] Korea Astron & Space Sci Inst, Solar & Space Weather Res Grp, Taejon 305348, South Korea.
[Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea.
[Moon, Y. -J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kudela, K.] Slovak Acad Sci, Inst Expt Phys, Kosice 04001, Slovakia.
[Dorman, L. I.] Russian Acad Sci, Cosm Ray Dept, Moscow 142190, Russia.
RP Firoz, KA (reprint author), Korea Astron & Space Sci Inst, Solar & Space Weather Res Grp, Taejon 305348, South Korea.
EM kazifiroz2002@gmail.com
RI Moon, Yong-Jae/E-1711-2013
FU Development of Korean Space Weather Center of Korea Astronomy and Space
Science Institute (KASI); KASI; VEGA [2/0081/10]; NASA [NNX10AL50A];
Ministry of Education, Science and Technology [R31-10016]; Korean
government (MOEHRD) [20090071744, 20100014501]
FX This work has been financed by the Development of Korean Space Weather
Center of Korea Astronomy and Space Science Institute (KASI) and KASI
basic research funds. K. Kudela wishes to acknowledge VEGA Project
2/0081/10. Data of the space satellites of GOES of NGDC, NOAA, and NASA
and data of the neutron monitor at Oulu have been studied. We would like
to express our gratitude to Sung-Hong Park KASI and Dmitry Prokhorov of
KASI for important discussions. The authors are indebted to the
anonymous reviewers for their constructive comments and suggestions that
indeed helped to develop this paper. The authors also recall two
important discussions with Sung-Hong Park and Dmitry Prokhorov of KASI.
Y.-J. Moon is supported by NASA grant (NNX10AL50A); by the WCU Program
(R31-10016) through the National Research Foundation of the Republic of
Korea funded by the Ministry of Education, Science and Technology; and
by the Korea Research Foundation grant (20090071744 and 20100014501)
funded by the Korean government (MOEHRD, Basic Research Promotion Fund).
NR 54
TC 9
Z9 9
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR 1
PY 2011
VL 116
AR A04101
DI 10.1029/2010JA016171
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 744HD
UT WOS:000289084600004
ER
PT J
AU Ukwatta, TN
Dhuga, KS
Morris, DC
MacLachlan, G
Parke, WC
Maximon, LC
Eskandarian, A
Gehrels, N
Norris, JP
Shenoy, A
AF Ukwatta, T. N.
Dhuga, K. S.
Morris, D. C.
MacLachlan, G.
Parke, W. C.
Maximon, L. C.
Eskandarian, A.
Gehrels, N.
Norris, J. P.
Shenoy, A.
TI A new frequency-luminosity relation for long gamma-ray bursts?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-ray burst: general
ID ALERT TELESCOPE; PEAK LUMINOSITY; VARIABILITY; SPECTRA; ESTIMATOR;
MISSION; SAMPLE; BAT
AB We have studied power density spectra (PDS) of 206 long gamma-ray bursts. We fitted the PDS with a simple power law and extracted the exponent of the power law (alpha) and the noise-crossing threshold frequency (f(th)). We find that the distribution of the extracted alpha peaks around -1.4 and that of f(th) around 1 Hz. In addition, based on a subset of 58 bursts with known redshifts, we show that the redshift-corrected threshold frequency is positively correlated with the isotropic peak luminosity. The correlation coefficient is 0.57 +/- 0.03.
C1 [Ukwatta, T. N.; Dhuga, K. S.; Morris, D. C.; MacLachlan, G.; Parke, W. C.; Maximon, L. C.; Eskandarian, A.; Shenoy, A.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
[Ukwatta, T. N.; Morris, D. C.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Norris, J. P.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
RP Ukwatta, TN (reprint author), George Washington Univ, Dept Phys, Washington, DC 20052 USA.
EM tilan.ukwatta@gmail.com
RI Gehrels, Neil/D-2971-2012
FU NASA [NNX08AR44A]
FX We thank the anonymous referee for comments and suggestions that
significantly improved the paper. We also thank T. Sakamoto and C.
Guidorzi for useful discussions. The NASA grant NNX08AR44A provided
partial support for this work and is gratefully acknowledged.
NR 22
TC 3
Z9 3
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 APR
PY 2011
VL 412
IS 2
BP 875
EP 882
DI 10.1111/j.1365-2966.2010.17944.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737DV
UT WOS:000288549900010
ER
PT J
AU Rowe, B
Silk, J
AF Rowe, Barnaby
Silk, Joseph
TI The Sunyaev-Zel'dovich effect due to hyperstarburst galaxy winds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE shock waves; galaxies: high-redshift; intergalactic medium; galaxies:
starburst
ID MOLECULAR GAS; GALACTIC WINDS; HIGH-REDSHIFT; HOST GALAXY; RELATIVISTIC
CORRECTIONS; ULTRALUMINOUS GALAXIES; SUBMILLIMETER GALAXIES; DISTANT
QUASARS; BIG-BANG; APEX-SZ
AB We construct a simple, spherical blast wave model to estimate the pressure structure of the intergalactic medium surrounding hyperstarburst galaxies, and argue that the effects of interaction with star-forming galaxy winds may be approximated at early times by an adiabatically expanding, self-similar 'bubble' as described by Weaver et al. and Ostriker & McKee. This model is used to make observational predictions for the thermal Sunyaev-Zel'dovich effect in the shocked bubble plasma. Radiative cooling losses are explored, and it is found that bremsstrahlung will limit the epoch of adiabatic expansion to 107- 108 yr: comparable to total hyperstarburst lifetimes. Prospects for making a first Sunyaev-Zel'dovich detection of galaxy wind bubbles using the Atacama Large Millimeter Array are examined for a number of active hyperstarburst sources in the literature.
C1 [Rowe, Barnaby] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rowe, Barnaby] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France.
[Silk, Joseph] Univ Oxford, Dept Phys, Oxford OX1 4LN, England.
RP Rowe, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM barnaby.t.rowe@jpl.nasa.gov
OI silk, joe/0000-0002-1566-8148; Rowe, Barnaby/0000-0002-7042-9174
FU European Union [MRTN-CT-2006-036133]
FX The authors would like to thank Richard Bielby, Arthur Kosowsky,
Vivienne Wild and the anonymous referee for useful comments and
suggestions. BR has been supported in part by the Dark Universe through
Extragalactic Lensing (DUEL) European Union FP6 Research Training
Network (MRTN-CT-2006-036133).
NR 59
TC 0
Z9 0
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 APR
PY 2011
VL 412
IS 2
BP 905
EP 910
DI 10.1111/j.1365-2966.2010.17953.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737DV
UT WOS:000288549900013
ER
PT J
AU Bracco, A
Cooray, A
Veneziani, M
Amblard, A
Serra, P
Wardlow, J
Thompson, MA
White, G
Auld, R
Baes, M
Bertoldi, F
Buttiglione, S
Cava, A
Clements, DL
Dariush, A
De Zotti, G
Dunne, L
Dye, S
Eales, S
Fritz, J
Gomez, H
Hopwood, R
Ibar, I
Ivison, RJ
Jarvis, M
Lagache, G
Lee, MG
Leeuw, L
Maddox, S
Michalowski, M
Pearson, C
Pohlen, M
Rigby, E
Rodighiero, G
Smith, DJB
Temi, P
Vaccari, M
van der Werf, P
AF Bracco, A.
Cooray, A.
Veneziani, M.
Amblard, A.
Serra, P.
Wardlow, J.
Thompson, M. A.
White, G.
Auld, R.
Baes, M.
Bertoldi, F.
Buttiglione, S.
Cava, A.
Clements, D. L.
Dariush, A.
De Zotti, G.
Dunne, L.
Dye, S.
Eales, S.
Fritz, J.
Gomez, H.
Hopwood, R.
Ibar, I.
Ivison, R. J.
Jarvis, M.
Lagache, G.
Lee, M. G.
Leeuw, L.
Maddox, S.
Michalowski, M.
Pearson, C.
Pohlen, M.
Rigby, E.
Rodighiero, G.
Smith, D. J. B.
Temi, P.
Vaccari, M.
van der Werf, P.
TI Herschel-ATLAS: statistical properties of Galactic cirrus in the GAMA-9
Hour Science Demonstration Phase Field
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: statistical; ISM: structure; infrared: ISM
ID TEMPERATURE-DEPENDENCE; SPECTRAL INDEX; ABSORPTION-COEFFICIENT; SPIRE
INSTRUMENT; NUMBER COUNTS; DUST EMISSION; MICRONS; NOISE; GRAINS; CORES
AB We study the spectral energy distribution (SED) and the power spectrum of Galactic cirrus emission observed in the 14 deg2 Science Demonstration Phase field of the Herschel-ATLAS using Herschel and IRAS data from 100 to 500 mu m. We compare the Spectral and Photometric Imaging Receiver (SPIRE) 250, 350 and 500 mu m maps with IRAS 100-mu m emission, binned in 6-arcmin pixels. We assume a modified blackbody SED with dust emissivity parameter beta (F proportional to lambda-beta) and a single dust temperature T-d, and find that the dust temperature and emissivity index varies over the science demonstration field as and 1 < beta < 4. The latter values are somewhat higher than the range of beta often quoted in the literature (1 < beta < 2). We estimate the mean values of these parameters to be T-d = 19.0 +/- 2.4 K and beta = 1.4 +/- 0.4. In regions of bright cirrus emission, we find that the dust has similar temperatures with , and similar values of beta, ranging from 1.4 +/- 0.5 to 1.9 +/- 0.5. We show that T-d and beta associated with diffuse cirrus emission are anti-correlated and can be described by the relationship: beta(T-d) = NT alpha(d) with [N = 116 +/- 38, alpha = -1.4 +/- 0.1]. The strong correlation found in this analysis is not just limited to high-density clumps of cirrus emission as seen in previous studies, but is also seen in diffuse cirrus in low-density regions. To provide an independent measure of T-d and beta, we obtain the angular power spectrum of the cirrus emission in the IRAS and SPIRE maps, which is consistent with a power spectrum of the form P(k) = P-0(k/k(0))gamma, where gamma = 2.6 +/- 0.2 for scales of 50-200 arcmin in the SPIRE maps. The cirrus rms fluctuation amplitude at angular scales of 100 arcmin is consistent with a modified blackbody SED with and beta = 1.3 +/- 0.2, in agreement with the values obtained above.
C1 [Bracco, A.; Cooray, A.; Veneziani, M.; Amblard, A.; Serra, P.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Cooray, A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Veneziani, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Thompson, M. A.; Jarvis, M.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[White, G.; Hopwood, R.; Pearson, C.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[White, G.] Rutherford Appleton Lab, Space Sci & Technol Div, Chilton OX11 0NL, Oxon, England.
[Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Gomez, H.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium.
[Bertoldi, F.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Buttiglione, S.; De Zotti, G.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Cava, A.] Univ La Laguna, Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain.
[Cava, A.] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Spain.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Dept Phys, London SW7 2AZ, England.
[De Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Dunne, L.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Ibar, I.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Michalowski, M.; van der Werf, P.] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Lagache, G.] Univ Paris 11, Lab IAS, UMR8617, F-91405 Orsay, France.
[Lagache, G.] CNRS, F-91405 Orsay, France.
[Lee, M. G.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Leeuw, L.] SETI Inst, Mountain View, CA 94043 USA.
[Pearson, C.] Rutherford Appleton Lab, Space Sci & Technol Dept, Chilton OX11 0QX, Oxon, England.
[Pearson, C.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada.
[Rodighiero, G.; Vaccari, M.] Univ Padua, Dept Astron, Padua, Italy.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Bracco, A (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
EM acooray@uci.edu
RI Baes, Maarten/I-6985-2013; Serra, Paolo/G-9678-2014; amblard,
alexandre/L-7694-2014; Wardlow, Julie/C-9903-2015; Ivison,
R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017;
OI Dye, Simon/0000-0002-1318-8343; Baes, Maarten/0000-0002-3930-2757;
Serra, Paolo/0000-0002-7609-3931; amblard,
alexandre/0000-0002-2212-5395; Wardlow, Julie/0000-0003-2376-8971;
Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577;
Cava, Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X;
Smith, Daniel/0000-0001-9708-253X; Rodighiero,
Giulia/0000-0002-9415-2296
FU NASA
FX The Herschel-ATLAS is a project with Herschel, which is an ESA space
observatory with science instruments provided by European-led Principal
Investigator consortia and with important participation from NASA. The
H-ATLAS website is http://www.h-atlas.org/. AA, AB, AC and PS
acknowledge support from NASA funds for US participants in Herschel
through JPL.
NR 51
TC 31
Z9 31
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2011
VL 412
IS 2
BP 1151
EP 1161
DI 10.1111/j.1365-2966.2010.17971.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737DV
UT WOS:000288549900034
ER
PT J
AU Braglia, FG
Ade, PAR
Bock, JJ
Chapin, EL
Devlin, MJ
Edge, A
Griffin, M
Gundersen, JO
Halpern, M
Hargrave, PC
Hughes, DH
Klein, J
Marsden, G
Mauskopf, P
Moncelsi, L
Netterfield, CB
Ngo, H
Olmi, L
Pascale, E
Patanchon, G
Pimbblet, KA
Rex, M
Scott, D
Semisch, C
Thomas, N
Truch, MDP
Tucker, C
Tucker, GS
Valiante, E
Viero, MP
Wiebe, DV
AF Braglia, Filiberto G.
Ade, Peter A. R.
Bock, James J.
Chapin, Edward L.
Devlin, Mark J.
Edge, Alastair
Griffin, Matthew
Gundersen, Joshua O.
Halpern, Mark
Hargrave, Peter C.
Hughes, David H.
Klein, Jeff
Marsden, Gaelen
Mauskopf, Philip
Moncelsi, Lorenzo
Netterfield, Calvin B.
Ngo, Henry
Olmi, Luca
Pascale, Enzo
Patanchon, Guillaume
Pimbblet, Kevin A.
Rex, Marie
Scott, Douglas
Semisch, Christopher
Thomas, Nicholas
Truch, Matthew D. P.
Tucker, Carole
Tucker, Gregory S.
Valiante, Elisabetta
Viero, Marco P.
Wiebe, Donald V.
TI Submillimetre observations of galaxy clusters with the BLAST: the star
formation activity in Abell 3112
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual: A3112;
galaxies: evolution; galaxies: star formation; infrared: galaxies;
submillimetre: galaxies
ID FAR-INFRARED EMISSION; STARBURST GALAXIES; INTRACLUSTER DUST; GALACTIC
NUCLEI; REDSHIFT SURVEY; HOST GALAXIES; RICH CLUSTERS; TO 0.3;
EVOLUTION; FIELD
AB We present observations at 250, 350 and 500 mu m of the nearby galaxy cluster Abell 3112 (z = 0.075) carried out with the Balloon-borne Large Aperture Submillimeter Telescope. Five cluster members are individually detected as bright submillimetre (submm) sources. Their far-infrared spectral energy distributions and optical colours identify them as normal star-forming galaxies of high mass, with globally evolved stellar populations. They all have (B - R) colours of 1.38 +/- 0.08, transitional between the blue, active population and the red, evolved galaxies that dominate the cluster core. We stack to estimate the mean submm emission from all cluster members, which is determined to be 16.6 +/- 2.5, 6.1 +/- 1.9 and 1.5 +/- 1.3 mJy at 250, 350 and 500 mu m, respectively. Stacking analyses of the submm emission of cluster members reveal trends in the mean far-infrared luminosity with respect to clustercentric radius and K-S-band magnitude. We find that a large fraction of submm emission comes from the boundary of the inner, virialized region of the cluster, at clustercentric distances around R-500. Stacking also shows that the bulk of the submm emission arises in intermediate-mass galaxies with K-S magnitude similar to 1 mag fainter than the giant ellipticals. The results and constraints obtained in this work will provide a useful reference for the forthcoming surveys to be conducted on galaxy clusters by Herschel.
C1 [Braglia, Filiberto G.; Chapin, Edward L.; Halpern, Mark; Marsden, Gaelen; Ngo, Henry; Scott, Douglas; Valiante, Elisabetta; Wiebe, Donald V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Moncelsi, Lorenzo; Pascale, Enzo; Tucker, Gregory S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Bock, James J.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Devlin, Mark J.; Klein, Jeff; Semisch, Christopher; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Edge, Alastair] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Gundersen, Joshua O.; Thomas, Nicholas] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Hughes, David H.] INAOE, Puebla 72000, Mexico.
[Netterfield, Calvin B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Olmi, Luca] Univ Puerto Rico, Phys Dept, UPR Stn, Rio Piedras, PR 00931 USA.
[Olmi, Luca] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Patanchon, Guillaume] Univ Paris Diderot, Lab APC, F-75205 Paris, France.
[Pimbblet, Kevin A.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Rex, Marie] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Tucker, Carole] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Viero, Marco P.] CALTECH, Pasadena, CA 91125 USA.
RP Braglia, FG (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
EM fbraglia@phas.ubc.ca
RI Klein, Jeffrey/E-3295-2013;
OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840;
Edge, Alastair/0000-0002-3398-6916; Ngo, Henry/0000-0001-5172-4859
FU National Aeronautics and Space Administration (NASA) [NAG5-12785,
NAG5-13301, NNGO-6GI11G]; NSF Office of Polar Programs; Canadian Space
Agency; Natural Sciences and Engineering Research Council (NSERC) of
Canada; UK Science and Technology Facilities Council (STFC); National
Science Foundation
FX We acknowledge the support of the National Aeronautics and Space
Administration (NASA) through grant numbers NAG5-12785, NAG5-13301 and
NNGO-6GI11G, the NSF Office of Polar Programs, the Canadian Space
Agency, the Natural Sciences and Engineering Research Council (NSERC) of
Canada, and the UK Science and Technology Facilities Council (STFC).
This research has been enabled by the use of WestGrid computing
resources. FGB acknowledges Daniele Pierini for helpful discussions and
the anonymous referee for their suggestions. This work is partly based
on observations made at the Australian Astronomical Observatory with the
Anglo-Australian Telescope. This research has made use of the NED, which
is operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the NASA. This publication makes use of
data products from the 2MASS, which is a joint project of the University
of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the NASA and the
National Science Foundation. 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 the NASA.
NR 73
TC 9
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U1 0
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2011
VL 412
IS 2
BP 1187
EP 1202
DI 10.1111/j.1365-2966.2010.17973.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737DV
UT WOS:000288549900037
ER
PT J
AU Leaman, J
Li, WD
Chornock, R
Filippenko, AV
AF Leaman, Jesse
Li, Weidong
Chornock, Ryan
Filippenko, Alexei V.
TI Nearby supernova rates from the Lick Observatory Supernova Search - I.
The methods and data base
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE surveys; supernovae: general; galaxies: evolution
ID CORE-COLLAPSE SUPERNOVAE; AUTOMATIC IMAGING TELESCOPE;
HUBBLE-SPACE-TELESCOPE; GAMMA-RAY BURSTS; IA SUPERNOVAE; HOST GALAXIES;
RELATIVE FREQUENCIES; STAR-FORMATION; HIGH-REDSHIFT; MASSIVE STAR
AB This is the first paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search. We have obtained 2.3 million observations of 14 882 sample galaxies over an interval of 11 years (1998 March to 2008 December). We considered 1036 SNe detected in our sample and used an optimal subsample of 726 SNe (274 Type Ia SNe, 116 Type Ibc SNe and Type II 324 SNe) to determine our SN rates. This is the largest and most homogeneous set of nearby SNe ever assembled for this purpose, and ours is the first local SN rate analysis based on CCD imaging and modern image-subtraction techniques. In this paper, we lay the foundation of the study. We derive the recipe for the control-time calculation for SNe with a known luminosity function and provide details on the construction of the galaxy and SN samples used in the calculations. Compared with a complete volume-limited galaxy sample, our sample has a deficit of low-luminosity galaxies but still provides enough statistics for a reliable rate calculation. There is a strong Malmquist bias, so the average size (luminosity or mass) of the galaxies increases monotonically with distance, and this trend is used to showcase a correlation between SN rates and galaxy sizes. Very few core-collapse SNe are found in early-type galaxies, providing strong constraints on the amount of recent star formation within these galaxies. The small average observation interval (similar to 9 d) of our survey ensures that our control-time calculations can tolerate a reasonable amount of uncertainty in the luminosity functions of SNe. We perform Monte Carlo simulations to determine the limiting magnitude of each image and the SN detection efficiency as a function of galaxy Hubble type. The limiting magnitude and the detection efficiency, together with the luminosity function derived from a complete sample of very nearby SNe in Paper II, will be used to calculate the control time and the SN rates in Paper III.
C1 [Leaman, Jesse; Li, Weidong; Chornock, Ryan; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA.
[Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Leaman, J (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM jleaman@astro.berkeley.edu; wli@astro.berkeley.edu;
rchornock@cfa.harvard.edu; alex@astro.berkeley.edu
FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO
Foundation; US Department of Energy [DE-FC02-06ER41453,
DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company;
AutoScope Corporation; Lick Observatory; NSF; University of California;
Sylvia & Jim Katzman Foundation; Richard and Rhoda Goldman Fund; NASA
FX The LOSS, conducted by AVF's group, has been supported by many grants
from the US National Science Foundation (NSF; most recently AST-0607485
and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC
grant DE-FC02-06ER41453 and US Department of Energy grant
DE-FG02-08ER41563. The KAIT and its ongoing operation were made possible
by donations from Sun Microsystems, Inc., the Hewlett-Packard Company,
AutoScope Corporation, Lick Observatory, the NSF, the University of
California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda
Goldman Fund and the TABASGO Foundation. We particularly thank Russell
M. Genet, who made the KAIT possible with his initial special gift;
former Lick Director Joseph S. Miller, who allowed the KAIT to be placed
at the Lick Observatory and provided staff support; and the TABASGO
Foundation, without which this work would not have been completed. JL is
grateful for a fellowship from the NASA Postdoctoral Program. We made
use of the NED, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. We
acknowledge the use of the HyperLeda data base (http://leda.univ-lyon1.
fr).
NR 123
TC 72
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U1 0
U2 1
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 APR
PY 2011
VL 412
IS 3
BP 1419
EP 1440
DI 10.1111/j.1365-2966.2011.18158.x
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745IM
UT WOS:000289159100002
ER
PT J
AU Li, WD
Leaman, J
Chornock, R
Filippenko, AV
Poznanski, D
Ganeshalingam, M
Wang, XF
Modjaz, M
Jha, S
Foley, RJ
Smith, N
AF Li, Weidong
Leaman, Jesse
Chornock, Ryan
Filippenko, Alexei V.
Poznanski, Dovi
Ganeshalingam, Mohan
Wang, Xiaofeng
Modjaz, Maryam
Jha, Saurabh
Foley, Ryan J.
Smith, Nathan
TI Nearby supernova rates from the Lick Observatory Supernova Search - II.
The observed luminosity functions and fractions of supernovae in a
complete sample
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE supernovae: general
ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURST; IA SUPERNOVAE; LIGHT CURVES;
HOST GALAXIES; INFRARED OBSERVATIONS; RELATIVE FREQUENCIES;
PHYSICAL-PROPERTIES; UBVRI PHOTOMETRY; SHOCK BREAKOUT
AB This is the second paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search (LOSS). In this paper, a complete SN sample is constructed, and the observed (uncorrected for host-galaxy extinction) luminosity functions (LFs) of SNe are derived. These LFs solve two issues that have plagued previous rate calculations for nearby SNe: the luminosity distribution of SNe and the host-galaxy extinction. We select a volume-limited sample of 175 SNe, collect photometry for every object and fit a family of light curves to constrain the peak magnitudes and light-curve shapes. The volume-limited LFs show that they are not well represented by a Gaussian distribution. There are notable differences in the LFs for galaxies of different Hubble types (especially for SNe Ia). We derive the observed fractions for the different subclasses in a complete SN sample, and find significant fractions of SNe II-L (10 per cent), IIb (12 per cent) and IIn (9 per cent) in the SN II sample. Furthermore, we derive the LFs and the observed fractions of different SN subclasses in a magnitude-limited survey with different observation intervals, and find that the LFs are enhanced at the high-luminosity end and appear more 'standard' with smaller scatter, and that the LFs and fractions of SNe do not change significantly when the observation interval is shorter than 10 d. We also discuss the LFs in different galaxy sizes and inclinations, and for different SN subclasses. Some notable results are that there is not a strong correlation between the SN LFs and the host-galaxy size, but there might be a preference for SNe IIn to occur in small, late-type spiral galaxies. The LFs in different inclination bins do not provide strong evidence for extreme extinction in highly inclined galaxies, though the sample is still small. The LFs of different SN subclasses show significant differences. We also find that SNe Ibc and IIb come from more luminous galaxies than SNe II-P, while SNe IIn come from less luminous galaxies, suggesting a possible metallicity effect. The limitations and applications of our LFs are also discussed.
C1 [Li, Weidong; Leaman, Jesse; Chornock, Ryan; Filippenko, Alexei V.; Poznanski, Dovi; Ganeshalingam, Mohan; Wang, Xiaofeng; Modjaz, Maryam; Jha, Saurabh; Foley, Ryan J.; Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA.
[Chornock, Ryan; Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Wang, Xiaofeng] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
[Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China.
[Modjaz, Maryam] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Jha, Saurabh] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Li, WD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM wli@astro.berkeley.edu
RI Wang, Xiaofeng/J-5390-2015
FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO
Foundation; US Department of Energy [DE-FC02-06ER41453,
DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company;
AutoScope Corporation; Lick Observatory; NSF [AST-0205808, AST-0606772];
University of California; Sylvia & Jim Katzman Foundation; Richard and
Rhoda Goldman Fund; NASA; Einstein Fellowship; NSFC [10673007,
11073013]; China-973 Program [2009CB824800]; Miller Institute for Basic
Research in Science (UC Berkeley)
FX We thank the referee, Enrico Cappellaro, for useful comments and
suggestions which improved the paper. We are grateful to the many
students, postdocs and other collaborators who have contributed to the
Katzman Automatic Imaging Telescope and the Lick Observatory Supernova
Search over the past two decades, and to discussions concerning the
determination of supernova rates - especially Jack Borde, Frank Serduke,
Jeffrey Silverman, Thea Steele and Richard R. Treffers. We thank the
Lick Observatory staff for their assistance with the operation of KAIT.
LOSS, conducted by AVF's group, has been supported by many grants from
the US National Science Foundation (NSF; most recently AST-0607485 and
AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC
grant DE-FC02-06ER41453 and US Department of Energy grant
DE-FG02-08ER41563. KAIT and its ongoing operation were made possible by
donations from Sun Microsystems, Inc., the Hewlett-Packard Company,
AutoScope Corporation, Lick Observatory, the NSF, the University of
California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda
Goldman Fund and the TABASGO Foundation. We give particular thanks to
Russell M. Genet, who made KAIT possible with his initial special gift;
former Lick Director Joseph S. Miller, who allowed KAIT to be placed at
Lick Observatory and provided staff support; and the TABASGO Foundation,
without which this work would not have been completed. JL is grateful
for a fellowship from the NASA Postdoctoral Program. DP is supported by
an Einstein Fellowship. XW acknowledges NSFC grants (10673007, 11073013)
and the China-973 Program 2009CB824800. MM acknowledges NSF grants
AST-0205808 and AST-0606772, as well as the Miller Institute for Basic
Research in Science (UC Berkeley), for support during the time over
which part of this work was conducted. We made use of the NASA/IPAC
Extragalactic Data base (NED), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. We acknowledge use of the HyperLeda data base
(http://leda.univ-lyon1.fr).
NR 133
TC 277
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U1 0
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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 APR
PY 2011
VL 412
IS 3
BP 1441
EP 1472
DI 10.1111/j.1365-2966.2011.18160.x
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745IM
UT WOS:000289159100003
ER
PT J
AU Li, WD
Chornock, R
Leaman, J
Filippenko, AV
Poznanski, D
Wang, XF
Ganeshalingam, M
Mannucci, F
AF Li, Weidong
Chornock, Ryan
Leaman, Jesse
Filippenko, Alexei V.
Poznanski, Dovi
Wang, Xiaofeng
Ganeshalingam, Mohan
Mannucci, Filippo
TI Nearby supernova rates from the Lick Observatory Supernova Search - III.
The rate-size relation, and the rates as a function of galaxy Hubble
type and colour
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general
ID CORE-COLLAPSE SUPERNOVAE; AEGIS FIELD GALAXIES; IA SUPERNOVAE;
STAR-FORMATION; MASSIVE STARS; LEGACY SURVEY; HIGH-REDSHIFT;
PROGENITORS; POPULATIONS; LUMINOSITY
AB This is the third paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search (LOSS). We have considered a sample of similar to 1000 SNe and used an optimal subsample of 726 SNe (274 SNe Ia, 116 SNe Ibc and 324 SNe II) to determine our rates. We study the trend of the rates as a function of a few quantities available for our galaxy sample, such as luminosity in the B and K bands, stellar mass and morphological class. We discuss different choices (SN samples, input SN luminosity functions, inclination correction factors) and their effect on the rates and their uncertainties. A comparison between our SN rates and the published measurements shows that they are consistent with each other to within the uncertainties when the rate calculations are done in the same manner. Nevertheless, our data demonstrate that the rates cannot be adequately described by a single parameter using either galaxy Hubble types or B - K colours. A secondary parameter in galaxy 'size', expressed by luminosity or stellar mass, is needed to adequately describe the rates in the rate-size relation: the galaxies of smaller sizes have higher SN rates per unit mass or per unit luminosity. The trends of the SN rates in galaxies of different Hubble types and colours are discussed. We examine possible causes for the rate-size relation. Physically, such a relation for the core-collapse SNe is probably linked to the correlation between the specific star-formation rate and the galaxy sizes, but it is not clear whether the same link can be established for SNe Ia. We discuss the two-component ('tardy' and 'prompt') model for SN Ia rates, and find that the SN Ia rates in young stellar populations might have a strong correlation with the core-collapse SN rates. We derive volumetric rates for the different SN types [e.g. for SNe Ia, a rate of (0.301 +/- 0.062) x 10-4 SN Mpc-3 yr-1 at redshift 0] and compare them to the measurements at different redshifts. Finally, we estimate the SN rate for the Milky Way Galaxy to be 2.84 +/- 0.60 SNe per century (with a systematic uncertainty of a factor of similar to 2), consistent with published SN rates based on several different techniques.
C1 [Li, Weidong; Chornock, Ryan; Leaman, Jesse; Filippenko, Alexei V.; Poznanski, Dovi; Wang, Xiaofeng; Ganeshalingam, Mohan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA.
[Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Wang, Xiaofeng] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
[Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China.
[Mannucci, Filippo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
RP Li, WD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM wli@astro.berkeley.edu
RI Wang, Xiaofeng/J-5390-2015;
OI mannucci, filippo/0000-0002-4803-2381
FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO
Foundation; US Department of Energy [DE-FC02-06ER41453,
DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company;
AutoScope Corporation; Lick Observatory; NSF; University of California;
Sylvia & Jim Katzman Foundation; Richard and Rhoda Goldman Fund; NASA;
Einstein Fellowship; NSFC [10673007, 11073013]; China-973 Program
[2009CB824800]
FX The LOSS, conducted by AVF's group, has been supported by many grants
from the US National Science Foundation (NSF; most recently AST-0607485
and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC
grant DE-FC02-06ER41453 and US Department of Energy grant
DE-FG02-08ER41563. The KAIT and its ongoing operation were made possible
by donations from Sun Microsystems, Inc., the Hewlett-Packard Company,
AutoScope Corporation, Lick Observatory, the NSF, the University of
California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda
Goldman Fund and the TABASGO Foundation. We give particular thanks to
Russell M. Genet, who made the KAIT possible with his initial special
gift; former Lick Director Joseph S. Miller, who allowed the KAIT to be
placed at Lick Observatory and provided staff support; and the TABASGO
Foundation, without which this work would not have been completed. JL is
grateful for a fellowship from the NASA Postdoctoral Program. DP is
supported by an Einstein Fellowship. XW acknowledges NSFC grants
(10673007, 11073013) and the China-973 Program 2009CB824800. We made use
of the NASA/IPAC Extragalactic Data base (NED), which is operated by the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. We acknowledge use of the HyperLeda data base
(http://leda.univlyon1.fr).
NR 58
TC 199
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U1 1
U2 9
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 APR
PY 2011
VL 412
IS 3
BP 1473
EP 1507
DI 10.1111/j.1365-2966.2011.18162.x
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745IM
UT WOS:000289159100004
ER
PT J
AU Starling, RLC
Evans, PA
Read, AM
Saxton, RD
Esquej, P
Krimm, H
O'Brien, PT
Osborne, JP
Mateos, S
Warwick, R
Wiersema, K
AF Starling, R. L. C.
Evans, P. A.
Read, A. M.
Saxton, R. D.
Esquej, P.
Krimm, H.
O'Brien, P. T.
Osborne, J. P.
Mateos, S.
Warwick, R.
Wiersema, K.
TI Swift follow-up of unidentified X-ray sources in the XMM-Newton Slew
Survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; X-rays: general
ID NORTH ECLIPTIC POLE; CHANDRA DEEP SURVEY; SKY SURVEY;
ULTRAVIOLET/OPTICAL TELESCOPE; SPECTRAL PROPERTIES; SOURCE CATALOG;
FIELD; BAT; CALIBRATION; MISSION
AB We present deep Swift follow-up observations of a sample of 94 unidentified X-ray sources from the XMM-Newton Slew Survey. The X-ray Telescope (XRT) on-board Swift detected 29 per cent of the sample sources; the flux limits for undetected sources suggest the bulk of the Slew Survey sources are drawn from one or more transient populations. We report revised X-ray positions for the XRT-detected sources, with typical uncertainties of 2.9 arcsec, reducing the number of catalogued optical matches to just a single source in most cases. We characterize the sources detected by Swift through their X-ray spectra and variability and via Ultraviolet-Optical Telescope photometry and using catalogued near-infrared, optical and radio observations of potential counterparts. Six sources can be associated with known objects and eight sources may be associated with unidentified ROSAT sources within the 3 Sigma error radii of our revised X-ray positions. We find 10 of the 30 XRT- and/or Burst Alert Telescope (BAT)-detected sources are clearly stellar in nature, including one periodic variable star and two high proper motion stars. For 11 sources we propose an active galactic nucleus (AGN) classification, among which four are detected in hard X-rays and three have redshifts spanning z = 0.2-0.9 obtained from the literature or from optical spectroscopy presented here. A further three sources are suspected AGN and one is a candidate Galactic hard X-ray flash, while five sources remain unclassified. The 67 Slew Survey sources we do not detect with Swift XRT or BAT are studied via their characteristics in the Slew Survey observations and by comparison with the XRT- and BAT-detected population. We suggest that these are mostly if not all extragalactic, though unlikely to be highly absorbed sources in the X-rays such as Compton thick AGN. A large number of these are highly variable soft X-ray (0.2-2 keV) sources and a smaller number are highly variable hard (2-12 keV) sources. A small fraction of mainly hard-band Slew Survey detections may be spurious. This follow-up programme brings us a step further to completing the identifications of a substantial sample of XMM-Newton Slew Survey sources, important for understanding the nature of the transient sky and allowing flux-limited samples to be constructed.
C1 [Starling, R. L. C.; Evans, P. A.; Read, A. M.; Esquej, P.; O'Brien, P. T.; Osborne, J. P.; Mateos, S.; Warwick, R.; Wiersema, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Saxton, R. D.] ESAC, XMM Newton SOC, Madrid 28691, Spain.
[Krimm, H.] Univ Space Res Assoc, Columbia, MD 20144 USA.
[Krimm, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Starling, RLC (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM rlcs1@star.le.ac.uk
RI Mateos, Silvia/F-9524-2016
OI Mateos, Silvia/0000-0002-1375-2389
FU STFC; National Aeronautics and Space Administration; National Science
Foundation
FX RLCS, PAE, AMR, PE and JPO acknowledge financial support from STFC. We
thank the Swift team for performing these observations. We acknowledge
useful discussions with S. Farrell and M. Goad and the anonymous referee
for a constructive critique. This work made use of data supplied by the
UK Swift Science Data Centre at the University of Leicester. 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. Based on observations obtained at
the ESO NTT telescope (programme 084.A-0828).
NR 58
TC 5
Z9 5
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2011
VL 412
IS 3
BP 1853
EP 1869
DI 10.1111/j.1365-2966.2010.18024.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745IM
UT WOS:000289159100034
ER
PT J
AU Zdziarski, AA
Pooley, GG
Skinner, GK
AF Zdziarski, Andrzej A.
Pooley, Guy G.
Skinner, Gerald K.
TI The doubling of the superorbital period of Cyg X-1
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: individual: Cyg X-1; stars:
individual: HDE 226868; radio continuum: stars; X-rays: binaries;
X-rays: stars
ID ALL-SKY MONITOR; WARPED ACCRETION DISCS; RAY TIMING EXPLORER; HDE
226868/CYG X-1; X-RAY; ORBITAL MODULATION; RADIO-EMISSION; TERM
VARIABILITY; SPACED DATA; CYG-X-1
AB We study properties of the superorbital modulation of the X-ray emission of Cyg X-1. We find that it has had a stable period of similar to 300 d in soft and hard X-rays and in radio since 2005 until at least 2010, which is about double the previously seen period. This new period, seen in the hard spectral state only, is detected not only in the light curves but also in soft X-ray hardness ratios and in the amplitude of the orbital modulation. On the other hand, the spectral slope in hard X-rays, greater than or similar to 20 keV, averaged over superorbital bins is constant, and the soft and hard X-rays and the radio emission change in phase. This shows that the superorbital variability consists of changing the normalization of an intrinsic spectrum of a constant shape and of changes of the absorbing column density with the phase. The maximum column density is achieved at the superorbital minimum. The amplitude changes are likely to be caused by a changing viewing angle of an anisotropic emitter, most likely a precessing accretion disc. The constant shape of the intrinsic spectrum shows that this modulation is not caused by a changing accretion rate. The modulated absorbing column density shows the presence of a bulge at the disc edge, as proposed previously. We also find the change of the superorbital period from similar to 150 to similar to 300 d to be associated with almost unchanged average X-ray fluxes, making the period change difficult to explain in the framework of disc-irradiation models. Finally, we find no correlation of the X-ray and radio properties with the reported detections in the GeV and TeV gamma-ray range.
C1 [Zdziarski, Andrzej A.] Ctr Astron M Kopernika, PL-00716 Warsaw, Poland.
[Pooley, Guy G.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Skinner, Gerald K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Skinner, Gerald K.] CRESST, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Skinner, Gerald K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Zdziarski, AA (reprint author), Ctr Astron M Kopernika, Bartycka 18, PL-00716 Warsaw, Poland.
EM aaz@camk.edu.pl
FU Polish MNiSW [NN203065933, 362/1/N-INTEGRAL/2008/09/0]; STFC
FX We thank A. Ogorzalek and L. Wen for help with calculating the rescaled
periodograms, H. Krimm and P. Lubinski for help with the BAT data, G.
Dubus for discussion of radiation induced precession and the referee for
valuable suggestions. This research has been supported in part by the
Polish MNiSW grants NN203065933 and 362/1/N-INTEGRAL/2008/09/0. The AMI
Arrays are operated by the University of Cambridge and supported by the
STFC. We acknowledge the use of data obtained through the HEASARC online
service provided by NASA/GSFC.
NR 53
TC 11
Z9 11
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 APR
PY 2011
VL 412
IS 3
BP 1985
EP 1992
DI 10.1111/j.1365-2966.2010.18034.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 745IM
UT WOS:000289159100044
ER
PT J
AU Brown, ME
Osgood, DE
Carriquiry, MA
AF Brown, Molly E.
Osgood, Daniel E.
Carriquiry, Miguel A.
TI Science-based insurance
SO NATURE GEOSCIENCE
LA English
DT Editorial Material
C1 [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Osgood, Daniel E.] Columbia Univ, Int Climate Res Inst Climate & Soc, Palisades, NY 10964 USA.
[Carriquiry, Miguel A.] Iowa State Univ, Ames, IA 50011 USA.
RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 614-4, Greenbelt, MD 20771 USA.
EM molly.brown@nasa.gov
RI Brown, Molly/M-5146-2013; Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314
NR 7
TC 10
Z9 10
U1 1
U2 10
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD APR
PY 2011
VL 4
IS 4
BP 213
EP 214
DI 10.1038/ngeo1117
PG 2
WC Geosciences, Multidisciplinary
SC Geology
GA 744AL
UT WOS:000289063900006
ER
PT J
AU Cuzzi, J
AF Cuzzi, Jeff
TI EARLY SOLAR SYSTEM Gathering dust
SO NATURE GEOSCIENCE
LA English
DT News Item
ID CHONDRULES; ACCRETION
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Cuzzi, J (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA.
EM Jeffrey.Cuzzi@nasa.gov
NR 6
TC 0
Z9 0
U1 1
U2 2
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD APR
PY 2011
VL 4
IS 4
BP 219
EP 220
DI 10.1038/ngeo1112
PG 2
WC Geosciences, Multidisciplinary
SC Geology
GA 744AL
UT WOS:000289063900009
ER
PT J
AU Alim, MA
Batra, AK
Aggarwal, MD
Currie, JR
AF Alim, Mohammad A.
Batra, A. K.
Aggarwal, M. D.
Currie, James R.
TI Immittance response of the SnO2-Bi2O3 based thick-films
SO PHYSICA B-CONDENSED MATTER
LA English
DT Article
DE Tin oxide; Binary oxides; Bismuth oxide; Impedance; Immittance
ID POLYCRYSTALLINE SOLID ELECTROLYTES; ZINC-OXIDE; SENSING PROPERTIES;
GRAIN-BOUNDARIES; VARISTORS; IMPEDANCE; BEHAVIOR; MICROSTRUCTURE;
CONDUCTIVITY; SPECTROSCOPY
AB The SnO2-Bi2O3 based thick-film polycrystalline material is fabricated on alumina substrate via screen-printing technique. This material system is evaluated at various temperatures (35 degrees C <= T <= 100 degrees C) using ac small-signal (immittance) measurements in the frequency range 10 Hz <= f <= 10(6) Hz. The simplistic analytical scenario for the immittance data employed the Cole-Cole empirical equation in conjunction with the estimation of the inspected input parameters. This is an alternate approach compared to the complex nonlinear least squares (CNLS) fitting procedure, and purely based on the appearance of the semicircular relaxation in the complex plane. It is found that the constituting components of the semicircular relaxation in the impedance plane are thermally activated indicating complexity in the grain boundary contributions despite the Debye and non-Debye relaxation responses. The possible degree of uniformity or non-uniformity in the grain boundary activity associated with its capacitance term observed via the Debye or non-Debye semicircular relaxation in the impedance (Z*) plane has been postulated. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Alim, Mohammad A.] Alabama A&M Univ, Dept Elect Engn, Huntsville, AL 35762 USA.
[Batra, A. K.; Aggarwal, M. D.] Alabama A&M Univ, Dept Phys, Normal, AL 35762 USA.
[Currie, James R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Alim, MA (reprint author), Alabama A&M Univ, Dept Elect Engn, POB 297, Huntsville, AL 35762 USA.
EM mohammad.alim@aamu.edu
FU NSF RISE [0927644]
FX The authors gratefully acknowledge the support of the present work
through NSF RISE grant no. 0927644. Thanks to Mr. G. Sharp for
fabrication of the sample holder and heater assembly.
NR 40
TC 1
Z9 1
U1 1
U2 17
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0921-4526
J9 PHYSICA B
JI Physica B
PD APR 1
PY 2011
VL 406
IS 8
BP 1445
EP 1452
DI 10.1016/j.physb.2011.01.046
PG 8
WC Physics, Condensed Matter
SC Physics
GA 743ZL
UT WOS:000289060100018
ER
PT J
AU Aihara, H
Prieto, CA
An, D
Anderson, SF
Aubourg, E
Balbinot, E
Beers, TC
Berlind, AA
Bickerton, SJ
Bizyaev, D
Blanton, MR
Bochanski, JJ
Bolton, AS
Bovy, J
Brandt, WN
Brinkmann, J
Brown, PJ
Brownstein, JR
Busca, NG
Campbell, H
Carr, MA
Chen, YM
Chiappini, C
Comparat, J
Connolly, N
Cortes, M
Croft, RAC
Cuesta, AJ
da Costa, LN
Davenport, JRA
Dawson, K
Dhital, S
Ealet, A
Ebelke, GL
Edmondson, EM
Eisenstein, DJ
Escoffier, S
Esposito, M
Evans, ML
Fan, XH
Castella, BF
Font-Ribera, A
Frinchaboy, PM
Ge, JA
Gillespie, BA
Gilmore, G
Hernandez, JIG
Gott, JR
Gould, A
Grebel, EK
Gunn, JE
Hamilton, JC
Harding, P
Harris, DW
Hawley, SL
Hearty, FR
Ho, S
Hogg, DW
Holtzman, JA
Honscheid, K
Inada, N
Ivans, II
Jiang, LH
Johnson, JA
Jordan, C
Jordan, WP
Kazin, EA
Kirkby, D
Klaene, MA
Knapp, GR
Kneib, JP
Kochanek, CS
Koesterke, L
Kollmeier, JA
Kron, RG
Lampeitl, H
Lang, D
Le Goff, JM
Lee, YS
Lin, YT
Long, DC
Loomis, CP
Lucatello, S
Lundgren, B
Lupton, RH
Ma, ZB
MacDonald, N
Mahadevan, S
Maia, MAG
Makler, M
Malanushenko, E
Malanushenko, V
Mandelbaum, R
Maraston, C
Margala, D
Masters, KL
McBride, CK
McGehee, PM
McGreer, ID
Menard, B
Miralda-Escude, J
Morrison, HL
Mullally, F
Muna, D
Munn, JA
Murayama, H
Myers, AD
Naugle, T
Neto, AF
Nguyen, DC
Nichol, RC
O'Connell, RW
Ogando, RLC
Olmstead, MD
Oravetz, DJ
Padmanabhan, N
Palanque-Delabrouille, N
Pan, K
Pandey, P
Paris, I
Percival, WJ
Petitjean, P
Pfaffenberger, R
Pforr, J
Phleps, S
Pichon, C
Pieri, MM
Prada, F
Price-Whelan, AM
Raddick, MJ
Ramos, BHF
Reyle, C
Rich, J
Richards, GT
Rix, HW
Robin, AC
Rocha-Pinto, HJ
Rockosi, CM
Roe, NA
Rollinde, E
Ross, AJ
Ross, NP
Rossetto, BM
Sanchez, AG
Sayres, C
Schlegel, DJ
Schlesinger, KJ
Schmidt, SJ
Schneider, DP
Sheldon, E
Shu, YP
Simmerer, J
Simmons, AE
Sivarani, T
Snedden, SA
Sobeck, JS
Steinmetz, M
Strauss, MA
Szalay, AS
Tanaka, M
Thakar, AR
Thomas, D
Tinker, JL
Tofflemire, BM
Tojeiro, R
Tremonti, CA
Vandenberg, J
Magana, MV
Verde, L
Vogt, NP
Wake, DA
Wang, J
Weaver, BA
Weinberg, DH
White, M
White, SDM
Yanny, B
Yasuda, N
Yeche, C
Zehavi, I
AF Aihara, Hiroaki
Allende Prieto, Carlos
An, Deokkeun
Anderson, Scott F.
Aubourg, Eric
Balbinot, Eduardo
Beers, Timothy C.
Berlind, Andreas A.
Bickerton, Steven J.
Bizyaev, Dmitry
Blanton, Michael R.
Bochanski, John J.
Bolton, Adam S.
Bovy, Jo
Brandt, W. N.
Brinkmann, J.
Brown, Peter J.
Brownstein, Joel R.
Busca, Nicolas G.
Campbell, Heather
Carr, Michael A.
Chen, Yanmei
Chiappini, Cristina
Comparat, Johan
Connolly, Natalia
Cortes, Marina
Croft, Rupert A. C.
Cuesta, Antonio J.
da Costa, Luiz N.
Davenport, James R. A.
Dawson, Kyle
Dhital, Saurav
Ealet, Anne
Ebelke, Garrett L.
Edmondson, Edward M.
Eisenstein, Daniel J.
Escoffier, Stephanie
Esposito, Massimiliano
Evans, Michael L.
Fan, Xiaohui
Femenia Castella, Bruno
Font-Ribera, Andreu
Frinchaboy, Peter M.
Ge, Jian
Gillespie, Bruce A.
Gilmore, G.
Gonzalez Hernandez, Jonay I.
Gott, J. Richard
Gould, Andrew
Grebel, Eva K.
Gunn, James E.
Hamilton, Jean-Christophe
Harding, Paul
Harris, David W.
Hawley, Suzanne L.
Hearty, Frederick R.
Ho, Shirley
Hogg, David W.
Holtzman, Jon A.
Honscheid, Klaus
Inada, Naohisa
Ivans, Inese I.
Jiang, Linhua
Johnson, Jennifer A.
Jordan, Cathy
Jordan, Wendell P.
Kazin, Eyal A.
Kirkby, David
Klaene, Mark A.
Knapp, G. R.
Kneib, Jean-Paul
Kochanek, C. S.
Koesterke, Lars
Kollmeier, Juna A.
Kron, Richard G.
Lampeitl, Hubert
Lang, Dustin
Le Goff, Jean-Marc
Lee, Young Sun
Lin, Yen-Ting
Long, Daniel C.
Loomis, Craig P.
Lucatello, Sara
Lundgren, Britt
Lupton, Robert H.
Ma, Zhibo
MacDonald, Nicholas
Mahadevan, Suvrath
Maia, Marcio A. G.
Makler, Martin
Malanushenko, Elena
Malanushenko, Viktor
Mandelbaum, Rachel
Maraston, Claudia
Margala, Daniel
Masters, Karen L.
McBride, Cameron K.
McGehee, Peregrine M.
McGreer, Ian D.
Menard, Brice
Miralda-Escude, Jordi
Morrison, Heather L.
Mullally, F.
Muna, Demitri
Munn, Jeffrey A.
Murayama, Hitoshi
Myers, Adam D.
Naugle, Tracy
Neto, Angelo Fausti
Duy Cuong Nguyen
Nichol, Robert C.
O'Connell, Robert W.
Ogando, Ricardo L. C.
Olmstead, Matthew D.
Oravetz, Daniel J.
Padmanabhan, Nikhil
Palanque-Delabrouille, Nathalie
Pan, Kaike
Pandey, Parul
Paris, Isabelle
Percival, Will J.
Petitjean, Patrick
Pfaffenberger, Robert
Pforr, Janine
Phleps, Stefanie
Pichon, Christophe
Pieri, Matthew M.
Prada, Francisco
Price-Whelan, Adrian M.
Raddick, M. Jordan
Ramos, Beatriz H. F.
Reyle, Celine
Rich, James
Richards, Gordon T.
Rix, Hans-Walter
Robin, Annie C.
Rocha-Pinto, Helio J.
Rockosi, Constance M.
Roe, Natalie A.
Rollinde, Emmanuel
Ross, Ashley J.
Ross, Nicholas P.
Rossetto, Bruno M.
Sanchez, Ariel G.
Sayres, Conor
Schlegel, David J.
Schlesinger, Katharine J.
Schmidt, Sarah J.
Schneider, Donald P.
Sheldon, Erin
Shu, Yiping
Simmerer, Jennifer
Simmons, Audrey E.
Sivarani, Thirupathi
Snedden, Stephanie A.
Sobeck, Jennifer S.
Steinmetz, Matthias
Strauss, Michael A.
Szalay, Alexander S.
Tanaka, Masayuki
Thakar, Aniruddha R.
Thomas, Daniel
Tinker, Jeremy L.
Tofflemire, Benjamin M.
Tojeiro, Rita
Tremonti, Christy A.
Vandenberg, Jan
Magana, M. Vargas
Verde, Licia
Vogt, Nicole P.
Wake, David A.
Wang, Ji
Weaver, Benjamin A.
Weinberg, David H.
White, Martin
White, Simon D. M.
Yanny, Brian
Yasuda, Naoki
Yeche, Christophe
Zehavi, Idit
TI THE EIGHTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST DATA FROM
SDSS-III
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE atlases; catalogs; surveys
ID SPECTROSCOPIC TARGET SELECTION; STAR-FORMING GALAXIES; 7TH DATA RELEASE;
OPEN CLUSTERS; WHITE-DWARFS; USNO-B; SEGUE; RESOLUTION; TELESCOPE;
CATALOG
AB The Sloan Digital Sky Survey (SDSS) started a new phase in 2008 August, with new instrumentation and new surveys focused on Galactic structure and chemical evolution, measurements of the baryon oscillation feature in the clustering of galaxies and the quasar Ly alpha forest, and a radial velocity search for planets around similar to 8000 stars. This paper describes the first data release of SDSS-III (and the eighth counting from the beginning of the SDSS). The release includes five-band imaging of roughly 5200 deg(2) in the southern Galactic cap, bringing the total footprint of the SDSS imaging to 14,555 deg(2), or over a third of the Celestial Sphere. All the imaging data have been reprocessed with an improved sky-subtraction algorithm and a final, self-consistent photometric recalibration and flat-field determination. This release also includes all data from the second phase of the Sloan Extension for Galactic Understanding and Exploration (SEGUE-2), consisting of spectroscopy of approximately 118,000 stars at both high and low Galactic latitudes. All the more than half a million stellar spectra obtained with the SDSS spectrograph have been reprocessed through an improved stellar parameter pipeline, which has better determination of metallicity for high-metallicity stars.
C1 [Bickerton, Steven J.; Carr, Michael A.; Gott, J. Richard; Gunn, James E.; Knapp, G. R.; Lang, Dustin; Loomis, Craig P.; Lupton, Robert H.; Mandelbaum, Rachel; Mullally, F.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Aihara, Hiroaki; Lin, Yen-Ting; Menard, Brice; Murayama, Hitoshi; Tanaka, Masayuki; Yasuda, Naoki] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Allende Prieto, Carlos; Esposito, Massimiliano; Femenia Castella, Bruno; Gonzalez Hernandez, Jonay I.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Allende Prieto, Carlos; Esposito, Massimiliano; Femenia Castella, Bruno] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[An, Deokkeun] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
[Anderson, Scott F.; Davenport, James R. A.; Evans, Michael L.; Hawley, Suzanne L.; Sayres, Conor; Schmidt, Sarah J.; Tofflemire, Benjamin M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Aubourg, Eric; Hamilton, Jean-Christophe; Magana, M. Vargas] Univ Paris Diderot, Astroparticule & Cosmol APC, F-75205 Paris 13, France.
[Aubourg, Eric; Le Goff, Jean-Marc; Palanque-Delabrouille, Nathalie; Rich, James; Yeche, Christophe] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France.
[Balbinot, Eduardo; Neto, Angelo Fausti] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil.
[Balbinot, Eduardo; Chiappini, Cristina; da Costa, Luiz N.; Maia, Marcio A. G.; Makler, Martin; Neto, Angelo Fausti; Ogando, Ricardo L. C.; Ramos, Beatriz H. F.; Rocha-Pinto, Helio J.; Rossetto, Bruno M.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, Brazil.
[Beers, Timothy C.; Lee, Young Sun] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Beers, Timothy C.; Lee, Young Sun] Michigan State Univ, Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA.
[Berlind, Andreas A.; Dhital, Saurav; McBride, Cameron K.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Bizyaev, Dmitry; Brinkmann, J.; Ebelke, Garrett L.; Gillespie, Bruce A.; Jordan, Cathy; Jordan, Wendell P.; Klaene, Mark A.; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Naugle, Tracy; Oravetz, Daniel J.; Pan, Kaike; Simmons, Audrey E.; Snedden, Stephanie A.] Apache Point Observ, Sunspot, NM 88349 USA.
[Blanton, Michael R.; Bovy, Jo; Hogg, David W.; Kazin, Eyal A.; Muna, Demitri; Price-Whelan, Adrian M.; Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Bochanski, John J.; Brandt, W. N.; Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Bolton, Adam S.; Brown, Peter J.; Brownstein, Joel R.; Dawson, Kyle; Harris, David W.; Ivans, Inese I.; Olmstead, Matthew D.; Pandey, Parul; Shu, Yiping; Simmerer, Jennifer] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Campbell, Heather; Edmondson, Edward M.; Lampeitl, Hubert; Maraston, Claudia; Masters, Karen L.; Nichol, Robert C.; Percival, Will J.; Pforr, Janine; Ross, Ashley J.; Thomas, Daniel; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Chen, Yanmei; Tremonti, Christy A.] Univ Wisconsin, Dept Astron, Madison, WI 53703 USA.
[Chiappini, Cristina; Steinmetz, Matthias] Astrophys Inst Potsdam, D-14482 Potsdam, Germany.
[Chiappini, Cristina] Ist Nazl Astrofis, I-34143 Trieste, Italy.
[Comparat, Johan; Kneib, Jean-Paul] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Connolly, Natalia] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA.
[Cortes, Marina; Ho, Shirley; Roe, Natalie A.; Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Croft, Rupert A. C.] Carnegie Mellon Univ, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Cuesta, Antonio J.; Lundgren, Britt; Padmanabhan, Nikhil; Wake, David A.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[da Costa, Luiz N.; Maia, Marcio A. G.; Ogando, Ricardo L. C.; Ramos, Beatriz H. F.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[Ealet, Anne; Escoffier, Stephanie] Aix Marseille Univ, CNRS, IN2P3, Ctr Phys Particules Marseille, Marseille, France.
[Ebelke, Garrett L.; Holtzman, Jon A.; Jordan, Wendell P.; Pfaffenberger, Robert; Vogt, Nicole P.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Eisenstein, Daniel J.; Fan, Xiaohui; Jiang, Linhua; McGreer, Ian D.; Szalay, Alexander S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Eisenstein, Daniel J.] Harvard Coll Observ, Cambridge, MA 02138 USA.
[Font-Ribera, Andreu] CSIC, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Frinchaboy, Peter M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA.
[Ge, Jian; Duy Cuong Nguyen; Wang, Ji] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA.
[Gilmore, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Gould, Andrew; Johnson, Jennifer A.; Kochanek, C. S.; Pieri, Matthew M.; Schlesinger, Katharine J.; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Grebel, Eva K.; Sivarani, Thirupathi] Univ Heidelberg, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Harding, Paul; Ma, Zhibo; Morrison, Heather L.; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
[Hearty, Frederick R.; O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Inada, Naohisa] Univ Tokyo, Grad Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan.
[Kirkby, David; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Koesterke, Lars] Univ Texas Austin, Texas Adv Comp Ctr, Austin, TX 78758 USA.
[Kollmeier, Juna A.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Kron, Richard G.; Yanny, Brian] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Kron, Richard G.; Sobeck, Jennifer S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Lucatello, Sara] INAF, Osservatorio Astrono Padova, I-35122 Padua, Italy.
[Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA.
[Makler, Martin] ICRA, Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, Brazil.
[McGehee, Peregrine M.] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Menard, Brice] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Menard, Brice; Raddick, M. Jordan; Szalay, Alexander S.; Thakar, Aniruddha R.; Vandenberg, Jan] Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Miralda-Escude, Jordi; Verde, Licia] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Miralda-Escude, Jordi; Verde, Licia] Univ Barcelona, IEEC, Inst Ciencies Cosmos, E-08028 Barcelona, Spain.
[Mullally, F.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Munn, Jeffrey A.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA.
[Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Paris, Isabelle; Petitjean, Patrick; Pichon, Christophe; Rollinde, Emmanuel] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France.
[Phleps, Stefanie; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Pieri, Matthew M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Reyle, Celine; Robin, Annie C.] Univ Franche Comte, Observ Besancon, Inst Utinam, F-25010 Besancon, France.
[Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
[Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Rocha-Pinto, Helio J.; Rossetto, Bruno M.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil.
[Rockosi, Constance M.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Sheldon, Erin] Bldg 510 Brookhaven Natl Lab Upton, Upton, NY 11973 USA.
[Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[White, Simon D. M.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
RP Strauss, MA (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RI Ho, Shirley/P-3682-2014; Balbinot, Eduardo/E-8019-2015; Padmanabhan,
Nikhil/A-2094-2012; Roe, Natalie/A-8798-2012; Yasuda, Naoki/A-4355-2011;
Aihara, Hiroaki/F-3854-2010; Kneib, Jean-Paul/A-7919-2015; Murayama,
Hitoshi/A-4286-2011; Le Goff, Jean-Marc/E-7629-2013; Tecnologias
espaciai, Inct/I-2415-2013; Gonzalez Hernandez, Jonay I./L-3556-2014;
Ogando, Ricardo/A-1747-2010; Mandelbaum, Rachel/N-8955-2014; Pforr,
Janine/J-3967-2015; Makler, Martin/G-2639-2012; White,
Martin/I-3880-2015; Brandt, William/N-2844-2015; Rocha-Pinto,
Helio/C-2719-2008; Jiang, Linhua/H-5485-2016; Croft, Rupert/N-8707-2014;
OI Ho, Shirley/0000-0002-1068-160X; Balbinot, Eduardo/0000-0002-1322-3153;
Aihara, Hiroaki/0000-0002-1907-5964; Kneib,
Jean-Paul/0000-0002-4616-4989; Gonzalez Hernandez, Jonay
I./0000-0002-0264-7356; Ogando, Ricardo/0000-0003-2120-1154; Mandelbaum,
Rachel/0000-0003-2271-1527; Cortes, Marina/0000-0003-0485-3767; Schmidt,
Sarah/0000-0002-7224-7702; Cuesta Vazquez, Antonio
Jose/0000-0002-4153-9470; Bovy, Jo/0000-0001-6855-442X; Verde,
Licia/0000-0003-2601-8770; /0000-0002-1891-3794; Masters,
Karen/0000-0003-0846-9578; Hogg, David/0000-0003-2866-9403; Davenport,
James/0000-0002-0637-835X; Pforr, Janine/0000-0002-3414-8391; Makler,
Martin/0000-0003-2206-2651; White, Martin/0000-0001-9912-5070; Brandt,
William/0000-0002-0167-2453; Jiang, Linhua/0000-0003-4176-6486; Croft,
Rupert/0000-0003-0697-2583; Kirkby, David/0000-0002-8828-5463;
Miralda-Escude, Jordi/0000-0002-2316-8370; Escoffier,
Stephanie/0000-0002-2847-7498
FU Alfred P. Sloan Foundation; National Science Foundation; US Department
of Energy; University of Arizona; Brazilian Participation Group;
Brookhaven National Laboratory; University of Cambridge; University of
Florida; French Participation Group; German Participation Group;
Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA
Participation Group; Johns Hopkins University; Lawrence Berkeley
National Laboratory; Max Planck Institute for Astrophysics; New Mexico
State University; New York University; Ohio State University;
Pennsylvania 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 We thank the referee, Andrew West, for comments that improved the paper.
Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the US Department of Energy. The SDSS-III Web site is
http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical
Research Consortium for the Participating Institutions of the SDSS-III
Collaboration including the University of Arizona, the Brazilian
Participation Group, Brookhaven National Laboratory, University of
Cambridge, University of Florida, the French Participation Group, the
German Participation Group, the Instituto de Astrofisica de Canarias,
the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins
University, Lawrence Berkeley National Laboratory, Max Planck Institute
for Astrophysics, New Mexico State University, New York University, Ohio
State University, Pennsylvania State University, University of
Portsmouth, Princeton University, the Spanish Participation Group,
University of Tokyo, University of Utah, Vanderbilt University,
University of Virginia, University of Washington, and Yale University.
NR 86
TC 725
Z9 731
U1 6
U2 53
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 APR
PY 2011
VL 193
IS 2
AR 29
DI 10.1088/0067-0049/193/2/29
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 743ZG
UT WOS:000289059200007
ER
PT J
AU Rebull, LM
Guieu, S
Stauffer, JR
Hillenbrand, LA
Noriega-Crespo, A
Stapelfeldt, KR
Carey, SJ
Carpenter, JM
Cole, DM
Padgett, DL
Strom, SE
Wolff, SC
AF Rebull, L. M.
Guieu, S.
Stauffer, J. R.
Hillenbrand, L. A.
Noriega-Crespo, A.
Stapelfeldt, K. R.
Carey, S. J.
Carpenter, J. M.
Cole, D. M.
Padgett, D. L.
Strom, S. E.
Wolff, S. C.
TI THE NORTH AMERICAN AND PELICAN NEBULAE. II. MIPS OBSERVATIONS AND
ANALYSIS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; infrared: ISM; infrared: stars; ISM: clouds; ISM:
individual objects (NGC 7000, IC 5070, LDN 935); stars: formation;
stars: pre-main sequence
ID SPITZER C2D SURVEY; MULTIBAND IMAGING PHOTOMETER; YOUNG STELLAR OBJECTS;
OPEN CLUSTER NGC-6996; STAR-FORMING REGIONS; EMISSION-LINE STARS; ARRAY
CAMERA IRAC; W-80 DARK CLOUD; ALL-SKY SURVEY; T-TAURI STARS
AB We present observations of similar to 7 deg(2) of the North American and Pelican Nebulae region at 24, 70, and 160 mu m with the Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS). We incorporate the MIPS observations with earlier Spitzer Infrared Array Camera (IRAC) observations, as well as archival near-infrared (IR) and optical data. We use the MIPS data to identify 1286 young stellar object (YSO) candidates. IRAC data alone can identify 806 more YSO candidates, for a total of 2076 YSO candidates. Prior to the Spitzer observations, there were only similar to 200 YSOs known in this region. Three subregions within the complex are highlighted as clusters: the Gulf of Mexico, the Pelican, and the Pelican's Hat. The Gulf of Mexico cluster is subject to the highest extinction (A(V) at least similar to 30) and has the widest range of infrared colors of the three clusters, including the largest excesses and by far the most point-source detections at 70 mu m. Just 3% of the cluster members were previously identified; we have redefined this cluster as about 10-100 times larger (in projected area) than was previously realized.
C1 [Rebull, L. M.; Stauffer, J. R.; Noriega-Crespo, A.; Carey, S. J.; Padgett, D. L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Guieu, S.] European So Observ, Santiago 19, Chile.
[Hillenbrand, L. A.; Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cole, D. M.] Raytheon Co, Pasadena, CA USA.
[Strom, S. E.; Wolff, S. C.] Natl Opt Astron Observ, Tucson, AZ USA.
RP Rebull, LM (reprint author), CALTECH, Spitzer Sci Ctr, M-S 220-6,1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM luisa.rebull@jpl.nasa.gov
OI Rebull, Luisa/0000-0001-6381-515X
FU National Aeronautics and Space Administration; National Science
Foundation; U.S. Government [NAG W-2166]
FX This research has made use of NASA's Astrophysics Data System (ADS)
Abstract Service, and of the SIMBAD database, operated at CDS,
Strasbourg, France. This research has made use of data products from the
Two Micron All-Sky Survey (2MASS), which is a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center, funded by the National Aeronautics and Space Administration and
the National Science Foundation. These data were served by the NASA/IPAC
Infrared Science Archive, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. This research has made
use of the Digitized Sky Surveys, which were produced at the Space
Telescope Science Institute under U.S. Government grant NAG W-2166. The
images of these surveys are based on photographic data obtained using
the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt
Telescope. The plates were processed into the present compressed digital
form with the permission of these institutions. This paper makes use of
data obtained as part of the INT Photometric Ha Survey of the Northern
Galactic Plane (IPHAS) carried out at the Isaac Newton Telescope (INT).
The INT 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. All IPHAS data, processed by the Cambridge
Astronomical Survey Unit, were obtained via the database and image
access provided by Astrogrid.
NR 86
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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 APR
PY 2011
VL 193
IS 2
AR 25
DI 10.1088/0067-0049/193/2/25
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 743ZG
UT WOS:000289059200003
ER
PT J
AU Tullmann, R
Gaetz, TJ
Plucinsky, PP
Kuntz, KD
Williams, BF
Pietsch, W
Haberl, F
Long, KS
Blair, WP
Sasaki, M
Winkler, PF
Challis, P
Pannuti, TG
Edgar, RJ
Helfand, DJ
Hughes, JP
Kirshner, RP
Mazeh, T
Shporer, A
AF Tuellmann, R.
Gaetz, T. J.
Plucinsky, P. P.
Kuntz, K. D.
Williams, B. F.
Pietsch, W.
Haberl, F.
Long, K. S.
Blair, W. P.
Sasaki, M.
Winkler, P. F.
Challis, P.
Pannuti, T. G.
Edgar, R. J.
Helfand, D. J.
Hughes, J. P.
Kirshner, R. P.
Mazeh, T.
Shporer, A.
TI THE CHANDRA ACIS SURVEY OF M33 (ChASeM33): THE FINAL SOURCE CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: general; galaxies: individual (M33); ISM: supernova remnants;
surveys; X-rays: galaxies
ID X-RAY SOURCES; STAR-FORMATION RATE; XMM-NEWTON SURVEY; LUMINOSITY
FUNCTION; SPIRAL GALAXIES; MILKY-WAY; SUPERNOVA-REMNANTS; PHOTOMETRIC
SURVEY; POINT SOURCES; SOURCE LIST
AB This study presents the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers similar to 70% of the D-25 isophote (R approximate to 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of similar to 2.4x10(34) erg s(-1) in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up MMT spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 is presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10(34) erg s(-1) and 1.6 x 10(35) erg s(-1)(for D = 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33.
C1 [Tuellmann, R.; Gaetz, T. J.; Plucinsky, P. P.; Challis, P.; Edgar, R. J.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kuntz, K. D.; Blair, W. P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Kuntz, K. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Williams, B. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Pietsch, W.; Haberl, F.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Long, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Sasaki, M.] Univ Tubingen, Inst Astron & Astrophys, Tubingen, Germany.
[Winkler, P. F.] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Pannuti, T. G.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA.
[Helfand, D. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Mazeh, T.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Shporer, A.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Tullmann, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rtuellmann@cfa.harvard.edu
RI Sasaki, Manami/P-3045-2016;
OI Sasaki, Manami/0000-0001-5302-1866; Haberl, Frank/0000-0002-0107-5237
FU National Aeronautics and Space Administration [G06-7073A]; National
Aeronautics Space and Administration [NAS8-03060]
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Number G06-7073A issued by the
Chandra X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory and on behalf of the National Aeronautics
Space and Administration under contract NAS8-03060. R.T., P.P.P.,
T.J.G., and R.J.E. acknowledge support under NASA contract NAS8-03060.
This work has made use of SAOImage DS9, developed by the Smithsonian
Astrophysical Observatory (Joye & Mandel 2003), the XSPEC spectral
fitting package (Arnaud 1996), the FUNTOOLS utilities package, the
HEASARC FTOOLS package, the CIAO (Chandra Interactive Analysis of
Observations) package, and ACIS Extract, the source extraction and
characterization tool developed and maintained by Pat Broos. Sincere
thanks to Pat Broos for answering our questions regarding AE and for
maintaining this important tool and to David Thilker for kindly
providing the Hi map of M33. We also acknowledge the heroic effort of
the anonymous referee for a careful reading of the manuscript and
several comments that helped to improve the paper.
NR 68
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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 APR
PY 2011
VL 193
IS 2
AR 31
DI 10.1088/0067-0049/193/2/31
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 743ZG
UT WOS:000289059200009
ER
PT J
AU Windhorst, RA
Cohen, SH
Hathi, NP
McCarthy, PJ
Ryan, RE
Yan, HJ
Baldry, IK
Driver, SP
Frogel, JA
Hill, DT
Kelvin, LS
Koekemoer, AM
Mechtley, M
O'Connell, RW
Robotham, ASG
Rutkowski, MJ
Seibert, M
Straughn, AN
Tuffs, RJ
Balick, B
Bond, HE
Bushouse, H
Calzetti, D
Crockett, M
Disney, MJ
Dopita, MA
Hall, DNB
Holtzman, JA
Kaviraj, S
Kimble, RA
MacKenty, JW
Mutchler, M
Paresce, F
Saha, A
Silk, JI
Trauger, JT
Walker, AR
Whitmore, BC
Young, ET
AF Windhorst, Rogier A.
Cohen, Seth H.
Hathi, Nimish P.
McCarthy, Patrick J.
Ryan, Russell E., Jr.
Yan, Haojing
Baldry, Ivan K.
Driver, Simon P.
Frogel, Jay A.
Hill, David T.
Kelvin, Lee S.
Koekemoer, Anton M.
Mechtley, Matt
O'Connell, Robert W.
Robotham, Aaron S. G.
Rutkowski, Michael J.
Seibert, Mark
Straughn, Amber N.
Tuffs, Richard J.
Balick, Bruce
Bond, Howard E.
Bushouse, Howard
Calzetti, Daniela
Crockett, Mark
Disney, Michael J.
Dopita, Michael A.
Hall, Donald N. B.
Holtzman, Jon A.
Kaviraj, Sugata
Kimble, Randy A.
MacKenty, John W.
Mutchler, Max
Paresce, Francesco
Saha, Abihit
Silk, Joseph I.
Trauger, John T.
Walker, Alistair R.
Whitmore, Bradley C.
Young, Erick T.
TI THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE
DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2-2 mu m WAVELENGTH
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE Galaxy: stellar content; infrared: galaxies; instrumentation: high
angular resolution; ultraviolet: galaxies
ID ULTRA-DEEP-FIELD; EMISSION-LINE GALAXIES; STAR-FORMATION HISTORY; LYMAN
BREAK GALAXIES; GOODS-SOUTH FIELD; HIGH-REDSHIFT GALAXIES; EXTREMELY RED
OBJECTS; NORTH GALACTIC POLE; MASS ASSEMBLY GAMA; TO 7 GALAXIES
AB We describe the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) Early Release Science (ERS) observations in the Great Observatories Origins Deep Survey (GOODS) South field. The new WFC3 ERS data provide calibrated, drizzled mosaics in the UV filters F225W, F275W, and F336W, as well as in the near-IR filters F098M (Y-s), F125W (J), and F160W (H) with 1-2 HST orbits per filter. Together with the existing HST Advanced Camera for Surveys (ACS) GOODS-South mosaics in the BViz filters, these panchromatic 10-band ERS data cover 40-50 arcmin(2) at 0.2-1.7 mu m in wavelength at 0 ''.07-0 ''.15 FWHM resolution and 0 ''.090 Multidrizzled pixels to depths of AB similar or equal to 26.0-27.0 mag (5 sigma) for point sources, and AB similar or equal to 25.5-26.5 mag for compact galaxies. In this paper, we describe (1) the scientific rationale, and the data taking plus reduction procedures of the panchromatic 10-band ERS mosaics, (2) the procedure of generating object catalogs across the 10 different ERS filters, and the specific star-galaxy separation techniques used, and (3) the reliability and completeness of the object catalogs from the WFC3 ERS mosaics. The excellent 0 ''.07-0 ''.15 FWHM resolution of HST/WFC3 and ACS makes star-galaxy separation straightforward over a factor of 10 in wavelength to AB similar or equal to 25-26 mag from the UV to the near-IR, respectively. Our main results are: (1) proper motion of faint ERS stars is detected over 6 years at 3.06 +/- 0.66 mas year(-1) (4.6 sigma), consistent with Galactic structure models; (2) both the Galactic star counts and the galaxy counts show mild but significant trends of decreasing count slopes from the mid-UV to the near-IR over a factor of 10 in wavelength; (3) combining the 10-band ERS counts with the panchromatic Galaxy and Mass Assembly survey counts at the bright end (10 mag less than or similar to AB less than or similar to 20 mag) and the Hubble Ultra Deep Field counts in the BVizY(s)JH filters at the faint end (24 mag less than or similar to AB less than or similar to 30 mag) yields galaxy counts that are well measured over the entire flux range 10 mag less than or similar to AB less than or similar to 30 mag for 0.2-2 mu m in wavelength; (4) simple luminosity+density evolution models can fit the galaxy counts over this entire flux range. However, no single model can explain the counts over this entire flux range in all 10 filters simultaneously. More sophisticated models of galaxy assembly are needed to reproduce the overall constraints provided by the current panchromatic galaxy counts for 10 mag less than or similar to AB less than or similar to 30 mag over a factor of 10 in wavelength.
C1 [Windhorst, Rogier A.; Cohen, Seth H.; Mechtley, Matt; Rutkowski, Michael J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Hathi, Nimish P.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[McCarthy, Patrick J.; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Ryan, Russell E., Jr.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Yan, Haojing] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Baldry, Ivan K.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Driver, Simon P.; Hill, David T.; Kelvin, Lee S.; Robotham, Aaron S. G.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Frogel, Jay A.] Assoc Univ Res Astron, Washington, DC 20005 USA.
[Koekemoer, Anton M.; Bond, Howard E.; Bushouse, Howard; MacKenty, John W.; Mutchler, Max; Whitmore, Bradley C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Straughn, Amber N.; Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tuffs, Richard J.] Max Planck Inst Nucl Phys MPIK, D-69117 Heidelberg, Germany.
[Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Calzetti, Daniela; Silk, Joseph I.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Crockett, Mark; Kaviraj, Sugata] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Disney, Michael J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Hall, Donald N. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Paresce, Francesco] INAF IASF Bologna, I-40129 Bologna, Italy.
[Saha, Abihit] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Trauger, John T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walker, Alistair R.] Cerro Tololo Interamer Observ, La Serena, Chile.
[Young, Erick T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Windhorst, RA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA.
EM Rogier.Windhorst@asu.edu
RI Robotham, Aaron/H-5733-2014; Dopita, Michael/P-5413-2014; Driver,
Simon/H-9115-2014; Hathi, Nimish/J-7092-2014;
OI Robotham, Aaron/0000-0003-0429-3579; Dopita,
Michael/0000-0003-0922-4986; Driver, Simon/0000-0001-9491-7327; Hathi,
Nimish/0000-0001-6145-5090; Mechtley, Matt/0000-0001-6462-6190;
Koekemoer, Anton/0000-0002-6610-2048
FU NASA through Space Telescope Science Institute [11359, GO-11359, NAS
5-26555]; NASA JWST, GSFC [NAG5-12460]; Center for Cosmology and
AstroParticle Physics (CCAPP) at The Ohio State University
FX Support for HST program 11359 was provided by NASA through grant
GO-11359 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. R.A.W. also acknowledges support from
NASA JWST Interdisciplinary Scientist grant NAG5-12460 from GSFC. H.Y.
is supported by the long-term fellowship program of the Center for
Cosmology and AstroParticle Physics (CCAPP) at The Ohio State
University.
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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 APR
PY 2011
VL 193
IS 2
AR 27
DI 10.1088/0067-0049/193/2/27
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 743ZG
UT WOS:000289059200005
ER
PT J
AU Kim, HS
Han, HD
Armaiz-Pena, GN
Stone, RL
Nam, EJ
Lee, JW
Shahzad, MMK
Nick, AM
Lee, SJ
Roh, JW
Nishimura, M
Mangala, LS
Bottsford-Miller, J
Gallick, GE
Lopez-Berestein, G
Sood, AK
AF Kim, Hye-Sun
Han, Hee Dong
Armaiz-Pena, Guillermo N.
Stone, Rebecca L.
Nam, Eun Ji
Lee, Jeong-Won
Shahzad, Mian M. K.
Nick, Alpa M.
Lee, Sun Joo
Roh, Ju-Won
Nishimura, Masato
Mangala, Lingegowda S.
Bottsford-Miller, Justin
Gallick, Gary E.
Lopez-Berestein, Gabriel
Sood, Anil K.
TI Functional Roles of Src and Fgr in Ovarian Carcinoma
SO CLINICAL CANCER RESEARCH
LA English
DT Article
ID FAMILY KINASES; CHITOSAN HYDROGEL; TYROSINE KINASE; CANCER CELLS; GENE
AMPLIFICATIONS; SIGNAL-TRANSDUCTION; PROSTATE-CANCER; MACROPHAGES;
INHIBITION; EXPRESSION
AB Purpose: Src is an attractive target because it is overexpressed in a number of malignancies, including ovarian cancer. However, the effect of Src silencing on other Src family kinases (SFKs) is not known. We hypothesized that other SFK members could compensate for the lack of Src activity.
Experimental Design: Cell viability after either Src or Fgr silencing was examined in ovarian cancer cell lines by MTT assay. Expression of SFKs after Src silencing in ovarian cancer cells was examined by real-time reverse transcriptase (RT)-PCR. Therapeutic effect of in vivo Src and/or Fgr silencing was examined using siRNA incorporated into chitosan nanoparticles (siRNA/CH-NP). Microvessel density, cell proliferation, and apoptosis markers were determined by immunohistochemical staining in ovarian tumor tissues.
Results: Src silencing enhanced cytotoxicity of docetaxel in both SKOV3ip1 and HeyA8 cells. In addition, Src silencing using siRNA/CH-NP in combination with docetaxel resulted in significant inhibition of tumor growth compared with control siRNA/CH-NP (81.8% reduction in SKOV3ip1, P = 0.017; 84.3% reduction in HeyA8, P < 0.005). These effects were mediated by decreased tumor cell proliferation and angiogenesis, and increased tumor cell apoptosis. Next, we assessed the effects of Src silencing on other SFK members in ovarian cancer cell lines. Src silencing resulted in significantly increased Fgr levels. Dual Src and Fgr silencing in vitro resulted in increased apoptosis that was mediated by increased caspase and AKT activity. In addition, dual silencing of Src and Fgr in vivo using siRNA/CH-NP resulted in the greatest reduction in tumor growth compared with silencing of either Src or Fgr alone in the HeyA8 model (68.8%, P < 0.05).
Conclusions: This study demonstrates that, in addition to Src, Fgr plays a biologically significant role in ovarian cancer growth and might represent an important target. Clin Cancer Res; 17(7); 1713-21. (C) 2011 AACR.
C1 [Kim, Hye-Sun; Han, Hee Dong; Armaiz-Pena, Guillermo N.; Stone, Rebecca L.; Nam, Eun Ji; Lee, Jeong-Won; Shahzad, Mian M. K.; Nick, Alpa M.; Lee, Sun Joo; Roh, Ju-Won; Nishimura, Masato; Mangala, Lingegowda S.; Bottsford-Miller, Justin; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Dept Gynecol Oncol, Houston, TX 77030 USA.
[Gallick, Gary E.] Univ Texas MD Anderson Canc Ctr, Dept Genitourinary Med Oncol, Houston, TX 77030 USA.
[Lopez-Berestein, Gabriel] Univ Texas MD Anderson Canc Ctr, Dept Expt Therapeut, Houston, TX 77030 USA.
[Lopez-Berestein, Gabriel; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Dept Canc Biol, Houston, TX 77030 USA.
[Han, Hee Dong; Lopez-Berestein, Gabriel; Sood, Anil K.] Univ Texas MD Anderson Canc Ctr, Ctr RNA Interference & Noncoding RNA, Houston, TX 77030 USA.
[Mangala, Lingegowda S.] NASA, Lyndon B Johnson Space Ctr, Dept Radiat Biophys, Univ Space Res Assoc, Houston, TX 77058 USA.
[Shahzad, Mian M. K.] Univ Wisconsin, Dept Obstet & Gynecol, Div Gynecol Oncol, Madison, WI 53706 USA.
[Shahzad, Mian M. K.] Univ Wisconsin, UW Carbone Canc Ctr, Madison, WI USA.
[Kim, Hye-Sun] Kwandong Univ, Coll Med, Womens Healthcare Ctr, Goyang, South Korea.
[Nam, Eun Ji] Yonsei Univ, Womens Canc Clin, Dept Obstet & Gynecol, Coll Med, Seoul 120749, South Korea.
[Lee, Jeong-Won] Sungkyunkwan Univ, Dept Obstet & Gynecol, Samsung Med Ctr, Sch Med, Seoul, South Korea.
[Lee, Sun Joo] Konkuk Univ, Dept Obstet & Gynecol, Konkuk Univ Hosp, Sch Med, Seoul, South Korea.
[Roh, Ju-Won] Dongguk Univ, Ilsan Hosp, Dept Obstet & Gynecol, Goyang, South Korea.
RP Sood, AK (reprint author), Univ Texas MD Anderson Canc Ctr, Dept Gynecol Oncol, 1155 Herman Pressler,Unit 1352, Houston, TX 77030 USA.
EM asood@mdanderson.org
RI lee, jw/O-6237-2014;
OI Armaiz-Pena, Guillermo N/0000-0002-9081-5339
FU NIH [CA 110793, 109298, CA 128797, RC2 GM 092599, U54 CA151668]; DOD
[OC-073399, W81 XWH-10-1-0158, BC 085265]; Ovarian Cancer Research Fund,
Inc.; U.T.M.D. Anderson Cancer Center SPORE [P50CA083639]; Zarrow
Foundation; Marcus Foundation; NCI-DHHS-NIH [T32 CA101642]; Baylor WRHR
[HD050128]; GCF Molly-Cade
FX Portions of this work were supported by NIH grants (CA 110793, 109298,
CA 128797, and RC2 GM 092599, U54 CA151668), DOD (OC-073399, W81
XWH-10-1-0158, BC 085265), the Ovarian Cancer Research Fund, Inc.
(Program Project Development Grant), U.T.M.D. Anderson Cancer Center
SPORE (P50CA083639), the Zarrow Foundation, the Marcus Foundation, the
Betty Anne Asche Murray Distinguished Professorship, and the Laura and
John Arnold Foundation. AMN, JBM, and RS are supported by NCI-DHHS-NIH
T32 Training Grant (T32 CA101642). MMS was supported by the Baylor WRHR
grant (HD050128) and the GCF Molly-Cade ovarian cancer research grant.
NR 30
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U1 0
U2 11
PU AMER ASSOC CANCER RESEARCH
PI PHILADELPHIA
PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA
SN 1078-0432
J9 CLIN CANCER RES
JI Clin. Cancer Res.
PD APR 1
PY 2011
VL 17
IS 7
BP 1713
EP 1721
DI 10.1158/1078-0432.CCR-10-2081
PG 9
WC Oncology
SC Oncology
GA 743XY
UT WOS:000289054100009
PM 21300758
ER
PT J
AU Mulavara, AP
Fiedler, MJ
Kofman, IS
Wood, SJ
Serrador, JM
Peters, B
Cohen, HS
Reschke, MF
Bloomberg, JJ
AF Mulavara, Ajitkumar P.
Fiedler, Matthew J.
Kofman, Igor S.
Wood, Scott J.
Serrador, Jorge M.
Peters, Brian
Cohen, Helen S.
Reschke, Millard F.
Bloomberg, Jacob J.
TI Improving balance function using vestibular stochastic resonance:
optimizing stimulus characteristics
SO EXPERIMENTAL BRAIN RESEARCH
LA English
DT Article
DE Stochastic resonance; Balance; Vestibular stimulation; Electrical
stimulation
ID HUMAN POSTURAL CONTROL; SENSORIMOTOR INTEGRATION; TACTILE SENSATION;
NOISE; STIMULATION; SYSTEM; MECHANORECEPTORS; SWAY; RESPONSES
AB Stochastic resonance (SR) is a phenomenon whereby the response of a non-linear system to a weak periodic input signal is optimized by the presence of a particular non-zero level of noise. Stochastic resonance using imperceptible stochastic vestibular electrical stimulation, when applied to normal young and elderly subjects, has been shown to significantly improve ocular stabilization reflexes in response to whole-body tilt; improved balance performance during postural disturbances and optimize covariance between the weak input periodic signals introduced via venous blood pressure receptors and the heart rate responses. In our study, 15 subjects stood on a compliant surface with their eyes closed. They were given low-amplitude binaural bipolar stochastic electrical stimulation of the vestibular organs in two frequency ranges of 1-2 and 0-30 Hz over the amplitude range of 0 to +/- 700 mu A. Subjects were instructed to maintain an upright stance during 43-s trials, which consisted of baseline (zero amplitude) and stimulation (non-zero amplitude) periods. Measures of stability of the head and trunk using inertial motion unit sensors attached to these segments and the whole body using a force plate were measured and quantified in the mediolateral plane. Using a multivariate optimization criterion, our results show that the low levels of vestibular stimulation given to the vestibular organs improved balance performance in normal healthy subjects in the range of 5-26% consistent with the stochastic resonance phenomenon. In our study, 8 of 15 and 10 of 15 subjects were responsive for the 1-2- and 0-30-Hz stimulus signals, respectively. The improvement in balance performance did not differ significantly between the stimulations in the two frequency ranges. The amplitude of optimal stimulus for improving balance performance was predominantly in the range of +/- 100 to +/- 400 mu A. A device based on SR stimulation of the vestibular system might be useful as either a training modality to enhance adaptability or skill acquisition, or as a miniature patch-type stimulator that may be worn by people with disabilities due to aging or disease to improve posture and locomotion function.
C1 [Mulavara, Ajitkumar P.; Wood, Scott J.] Univ Space Res Assoc, Houston, TX 77058 USA.
[Fiedler, Matthew J.; Kofman, Igor S.; Peters, Brian] Wyle Integrated Sci & Engn Grp, Houston, TX USA.
[Serrador, Jorge M.] NJ Healthcare Syst, Dept Vet Affairs, E Orange, NJ USA.
[Cohen, Helen S.] Baylor Coll Med, Houston, TX 77030 USA.
[Reschke, Millard F.; Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Mulavara, AP (reprint author), Univ Space Res Assoc, 2101 NASA Pkwy,Mail Code SK-B272, Houston, TX 77058 USA.
EM ajitkumar.p.mulavara@nasa.gov
FU National Space Biomedical Research Institute through NASA [NCC 9-58
(SA02001)]
FX This study was supported in part by a grant from the National Space
Biomedical Research Institute through NASA NCC 9-58 (SA02001) to
Ajitkumar Mulavara (PI). We would like to thank Erin Heap, Keena Acock,
and Elizabeth Fisher for their help with data analysis and data
collection and Hamish MacDougal and John Holden for their help with
design and building the vestibular stimulation system. We would also
like to thank all the subjects who participated voluntarily in the
experiments.
NR 47
TC 23
Z9 25
U1 1
U2 22
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0014-4819
EI 1432-1106
J9 EXP BRAIN RES
JI Exp. Brain Res.
PD APR
PY 2011
VL 210
IS 2
BP 303
EP 312
DI 10.1007/s00221-011-2633-z
PG 10
WC Neurosciences
SC Neurosciences & Neurology
GA 742QJ
UT WOS:000288959200014
PM 21442221
ER
PT J
AU Zwart, SR
Mehta, SK
Ploutz-Snyder, R
Liourbeau, Y
Locke, JP
Pierson, DL
Smith, SM
AF Zwart, Sara R.
Mehta, Satish K.
Ploutz-Snyder, Robert
Liourbeau, YaVonne
Locke, James P.
Pierson, Duane L.
Smith, Scott M.
TI Response to Vitamin D Supplementation during Antarctic Winter Is Related
to BMI, and Supplementation Can Mitigate Epstein-Barr Virus Reactivation
SO JOURNAL OF NUTRITION
LA English
DT Article
ID SPACE-FLIGHT; CALCIUM-METABOLISM; HEALTH; ASTRONAUTS; DISEASE;
SPACEFLIGHT; PERSPECTIVE; IMMUNITY; STATION; CANCER
AB Maintaining vitamin D status without sunlight exposure is difficult without supplementation. This study was designed to better understand interrelatiorships between periodic vitamin D supplementation and immune function n Antarctic workers. The effect of 2 oral dosing regimens of vitamin D supplementation on vitamin D status and markers of immune function was evaluated in people in Antarctica with no UV light exposure for 6 mo. Participants were given a 2000-IU (50 mu g) daily (n = 15) or 10.000 IU (250 mu g) weekly (n = 14) vitamin D supplement for 6 mo during a winter in Antarctica. Biological samples were collected at baseline and at 3 and 6 mo. Vitamin D intake, markers of vitamin D and bone metabolism. and latent virus reactivation were determined. After 6 mo, the serum 25-hydroxyvitamin D concentration (mean SD) increased from 56 +/- 17 to 79 +/- 16 mmol/L and from 52 = 10 to 60 +/- 9 nmol/1 in the 2000-IU/d and 10,000-IU/wk groups, respectively (main effect over time, P < 0.001). Participants with a greater BMI (participant BMI range = 19-43 g/m(2)) had a smaller increase in 25-hyd-oxyvitamin D after 6 mo supplementation (P < 0.05). Participants with high serum cortisol and higher serum 25-hydroxyvitamin D were less likely to shed Epstein Barr virus in saliva (P < 0.05). The aoses given raised vitamn D status in participants not exposed to sunlight for 6 mo, and the efficacy was influenced by baseline vitamin D status and BMI. The data also provide evidence trial vitamin D, interacting with stress, can reduce risk of latent virus reactivation during the winter in Antarctica. J. Nutr, 141: 692-697, 2011.
C1 [Locke, James P.; Pierson, Duane L.; Smith, Scott M.] NASA, Johnson Space Ctr, Space Life Sci Directorate, Houston, TX 77058 USA.
[Zwart, Sara R.; Ploutz-Snyder, Robert] Univ Space Res Assoc, Houston, TX 77058 USA.
[Mehta, Satish K.; Liourbeau, YaVonne] Enterprise Advisory Serv Inc, Houston, TX 77058 USA.
RP Smith, SM (reprint author), NASA, Johnson Space Ctr, Space Life Sci Directorate, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov
FU NASA; National Science Foundation
FX Supported by The NASA Human Research Program Human Health and
Countermeasures Element and made possible by the National Science
Foundation
NR 27
TC 28
Z9 28
U1 0
U2 5
PU AMER SOC NUTRITIONAL SCIENCE
PI BETHESDA
PA 9650 ROCKVILLE PIKE, RM L-2407A, BETHESDA, MD 20814 USA
SN 0022-3166
J9 J NUTR
JI J. Nutr.
PD APR
PY 2011
VL 141
IS 4
BP 692
EP 697
DI 10.3945/jn.110.134742
PG 6
WC Nutrition & Dietetics
SC Nutrition & Dietetics
GA 741PU
UT WOS:000288876800023
PM 21539011
ER
PT J
AU Ashour-Abdalla, M
El-Alaoui, M
Goldstein, ML
Zhou, M
Schriver, D
Richard, R
Walker, R
Kivelson, MG
Hwang, KJ
AF Ashour-Abdalla, Maha
El-Alaoui, Mostafa
Goldstein, Melvyn L.
Zhou, Meng
Schriver, David
Richard, Robert
Walker, Raymond
Kivelson, Margaret G.
Hwang, Kyoung-Joo
TI Observations and simulations of non-local acceleration of electrons in
magnetotail magnetic reconnection events
SO NATURE PHYSICS
LA English
DT Article
ID SUBSTORM ONSET; PARTICLE-ACCELERATION; THEMIS; MOTION; FIELDS
AB Magnetic reconnection in magnetized plasmas represents a change in magnetic field topology and is associated with a concomitant energization of charged particles that results from a conversion of magnetic energy into particle energy. In Earth's magnetosphere this process is associated with the entry of the solar wind into the magnetosphere and with the initiation of auroral substorms. Using data from the THEMIS mission, together with global and test particle simulations, we demonstrate that electrons are energized in two distinct regions: a low-energy population (less than or equal to a few kiloelectronvolts) that arises in a diffusion region where particles are demagnetized and the magnetic topology changes, and a high-energy component (approaching 100 keV) that results from betatron acceleration within dipolarization fronts that sweep towards the inner magnetosphere far from the diffusion region. Thus, the observed particle energization is associated with both magnetic reconnection and with betatron acceleration associated with macroscopic flows.
C1 [Ashour-Abdalla, Maha; El-Alaoui, Mostafa; Schriver, David; Richard, Robert; Walker, Raymond; Kivelson, Margaret G.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Goldstein, Melvyn L.; Hwang, Kyoung-Joo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhou, Meng] Nanchang Univ, Inst Space Sci & Technol, Nanchang 330031, Peoples R China.
[Kivelson, Margaret G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Hwang, Kyoung-Joo] Univ Maryland Baltimore Cty, Catonsville, MD 21250 USA.
RP Ashour-Abdalla, M (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
EM mabdalla@igpp.ucla.edu
RI Goldstein, Melvyn/B-1724-2008; Kivelson, Margaret/I-9019-2012; NASA MMS,
Science Team/J-5393-2013
OI Kivelson, Margaret/0000-0003-3859-8581; NASA MMS, Science
Team/0000-0002-9504-5214
FU NASA [NNX08AO48G, NAS5-02099, UCB NAS 5-02099]
FX We thank H. Kohne for help with programming and display of the data and
simulation results. Research at UCLA was supported by NASA grant
NNX08AO48G. 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 the use of ESA data, D. Larson and R. P. Lin for the
use of SST data, K. H. Glassmeier, U. Auster and W. Baumjohann for the
use of FGM data, J. W. Bonnell and F. S. Mozer for the use of EFI data,
and A. Roux and O. LeContel for the use of SCM data. K-J.H. and M. L. G.
were supported, in part, by NASA's Magnetospheric Multiscale and Cluster
missions at the Goddard Space Flight Center. M. G. K. was supported, in
part, by NASA Grant UCB NAS 5-02099. The computing was carried out on
NASA's Columbia Supercomputer.
NR 39
TC 81
Z9 82
U1 0
U2 8
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1745-2473
J9 NAT PHYS
JI Nat. Phys.
PD APR
PY 2011
VL 7
IS 4
BP 360
EP 365
DI 10.1038/NPHYS1903
PG 6
WC Physics, Multidisciplinary
SC Physics
GA 744DZ
UT WOS:000289076000025
ER
PT J
AU Vorotnikov, VS
Smith, CW
Farrugia, CJ
Meredith, CJ
Hu, QA
Szabo, A
Skoug, RM
Cohen, CMS
Davis, AJ
Yumoto, K
AF Vorotnikov, Vasiliy S.
Smith, Charles W.
Farrugia, Charles J.
Meredith, Calum J.
Hu, Qiang
Szabo, Adam
Skoug, Ruth M.
Cohen, Christina M. S.
Davis, Andrew J.
Yumoto, Kiyohumi
TI Use of single-component wind speed in Rankine-Hugoniot analysis of
interplanetary shocks
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID SOLAR-WIND
AB We have extended and deployed a routine designed to run independently on the Web providing real-time analysis of interplanetary shock observations from L(1). The program accesses real-time magnetic field, solar wind speed, and proton density data from the Advanced Composition Explorer (ACE) spacecraft, searches for interplanetary shocks, analyzes shocks according to the Rankine-Hugoniot (R-H) jump conditions, and provides shock solutions on the Web for space weather applications. Because the ACE real-time data stream contains the wind speed but not the three-component wind velocity, we describe modifications to the R-H analysis that use the scalar wind speed and show successful results for analyses of strong interplanetary shocks at 1 AU. We compare the three-component and one-component solutions and find the greatest disagreement between the two rests in estimations of the shock speed rather than the shock propagation direction. Uncertainties in magnetic quantities such as magnetic compression and shock normal angle relative to the upstream magnetic field show large uncertainties in both analyses when performed using an automated routine whereas analyses of the shock normal alone do not. The automated data point selection scheme, together with the natural variability of the magnetic field, is inferred to be a problem in a few instances for this and other reasons. For a broad range of interplanetary shocks that arrive 30 to 60 min after passing L(1), this method will provide 15 to 45 min of advanced warning prior to the shock's collision with the Earth's magnetopause. The shock, in turn, provides advance warning of the approaching driver gas.
C1 [Vorotnikov, Vasiliy S.] Univ New Hampshire, Dept Chem Engn, Durham, NH 03824 USA.
[Cohen, Christina M. S.; Davis, Andrew J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Smith, Charles W.; Farrugia, Charles J.] Univ New Hampshire, Ctr Space Sci, Inst Study Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA.
[Hu, Qiang] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Meredith, Calum J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Skoug, Ruth M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Szabo, Adam] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yumoto, Kiyohumi] Kyushu Univ, Space Environm Res Ctr, Fukuoka 8128581, Japan.
RP Vorotnikov, VS (reprint author), Univ New Hampshire, Dept Chem Engn, Durham, NH 03824 USA.
EM vasya@udel.edu; charles.smith@unh.edu; charlie.farrugia@unh.edu;
cjm49@leicester.ac.uk; qh0001@uah.edu; adam.szabo@nasa.gov;
rskoug@lanl.gov; cohen@srl.caltech.edu; ad@srl.caltech.edu;
yumoto@serc.kyushu-u.ac.jp
FU NASA [NNG04GMO5G, NAG5-12492]; Caltech [44A-1062037]; U.S. Department of
Energy
FX Funding for this work was provided by NASA grants NNG04GMO5G and
NAG5-12492 and Caltech subcontract 44A-1062037 in support of the ACE/MAG
experiment. Support at LANL was provided under the auspices of the U.S.
Department of Energy, with financial support from the NASA ACE program.
We thank the Solar-Terrestrial Laboratory at Nagoya University for
providing the 210MM magnetic observations and the IMAGE ground-based
magnetometer team for providing data used in this study. V. S. V. was an
undergraduate senior at UNH pursuing a chemical engineering major in
renewable energy when this work was performed. He is now a graduate
student in the Center for Renewable Energy at the University of
Delaware. C.J.M. was a visiting undergraduate at UNH at the time this
work was completed.
NR 14
TC 5
Z9 5
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR 1
PY 2011
VL 9
AR S04001
DI 10.1029/2010SW000631
PG 9
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 744KS
UT WOS:000289093900001
ER
PT J
AU Ari-Gur, P
Sariel, J
Stanford, MK
DellaCorte, C
Abel, PB
AF Ari-Gur, P.
Sariel, J.
Stanford, M. K.
DellaCorte, C.
Abel, P. B.
TI Phase identification of hard precipitates in PS304 coatings
SO SURFACE ENGINEERING
LA English
DT Article
DE PS304; Tribological coatings; X-ray diffraction
ID TEMPERATURE; STRENGTH
AB This paper presents the details of the detection of an unexpected (enigmatic) phase resulting from heat treatment of a tribocoating labelled PS304. This coating, consisting of chromium oxide powder in a Ni-Cr base powder and lubricated by silver metal and fluorides of barium and calcium, provides a plasma sprayed lubricious multitemperature wear and oxidation resistant surface layer for challenging wear applications. Primarily based on X-ray diffraction structural analysis, a chromium disilicide compound has been identified to form as a result of the heat treatment of the coating. A source of the significant strengthening of the coating by the heat treatment process is explained on the basis of the formation of the disilicide compound and its properties. The strengthening effect of fugitive silicon present in such trace levels is recognised for the first time as having a potential for use in many tribocoating systems as a cost effective and efficient strengthening approach.
C1 [Ari-Gur, P.] Western Michigan Univ, Dept Mech & Aeronaut Engn, Kalamazoo, MI 49008 USA.
[Sariel, J.] Nucl Res Ctr, Beer Sheva, Israel.
[Stanford, M. K.; DellaCorte, C.; Abel, P. B.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Ari-Gur, P (reprint author), Western Michigan Univ, Dept Mech & Aeronaut Engn, Kalamazoo, MI 49008 USA.
EM pnina.ari-gur@wmich.edu
NR 8
TC 1
Z9 1
U1 1
U2 7
PU MANEY PUBLISHING
PI LEEDS
PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND
SN 0267-0844
J9 SURF ENG
JI Surf. Eng.
PD APR
PY 2011
VL 27
IS 3
BP 196
EP 198
DI 10.1179/026708410X12683118611301
PG 3
WC Materials Science, Coatings & Films
SC Materials Science
GA 744GF
UT WOS:000289082200009
ER
PT J
AU Pinel, SI
Signer, HR
Zaretsky, EV
AF Pinel, Stanley I.
Signer, Hans R.
Zaretsky, Erwin V.
TI Comparison Between Oil-Mist and Oil-Jet Lubrication of High-Speed,
Small-Bore, Angular-Contact Ball Bearing
SO TRIBOLOGY & LUBRICATION TECHNOLOGY
LA English
DT Article
DE Rolling-Element Bearings; Ball Bearings; Life Prediction; Lubrication;
Oil-Jet Lubrication; Air-Oil Mist Lubrication
AB Parametric tests were conducted with an optimized 35-mm-bore-angular-contact ball bearing on a high-speed, high-temperature bearing tester Results from both air-oil mist lubrication and oil-jet lubrication systems used to lubricate the bearing were compared to speeds of 2.5Y10(6) DN. The maximum obtainable speed with air-oil mist lubrication is 2.5Y10(6) DN. Lower bearing temperatures and higher power losses are obtained with oil-jet lubrication than with air-oil mist lubrication Bearing power loss is a direct function of oil flow to the bearing and independent of oil delivery system. For a given oil-flow rate, bearing temperature and power loss increase with increases in speed. Bearing life is an inverse function of temperature, the difference in temperature between the individual bearing ring components, and the resultant elastohydrodynamic (EHD)film thicknesses. Bearing life is independent of the oil delivery system except as it affects temperature. Cage slip increased with increases in speed. Cage slip as high as 7 percent was measured and was generally higher with air-oil mist lubrication than with oil-jet lubrication.
C1 [Pinel, Stanley I.] Pinel Engn, Fullerton, CA 92821 USA.
[Signer, Hans R.] Signer Tech Serv, Fullerton, CA USA.
[Zaretsky, Erwin V.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Pinel, SI (reprint author), Pinel Engn, Fullerton, CA 92821 USA.
NR 13
TC 0
Z9 0
U1 1
U2 3
PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS
PI PARK RIDGE
PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA
SN 1545-858X
J9 TRIBOL LUBR TECHNOL
JI Tribol. Lubr. Technol.
PD APR
PY 2011
VL 67
IS 4
BP 32
EP 41
PG 10
WC Engineering, Mechanical
SC Engineering
GA 744WL
UT WOS:000289125800010
ER
PT J
AU Levit, C
Marshall, W
AF Levit, Creon
Marshall, William
TI Improved orbit predictions using two-line elements
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Space debris; Conjunction analysis; Orbit prediction
ID ACCURACY ASSESSMENT; SYSTEM; SATELLITES; PRECISION; CATALOG; LEO
AB The density of orbital space debris constitutes an increasing environmental challenge. There are two ways to alleviate the problem: debris mitigation and debris removal. This paper addresses collision avoidance, a key aspect of debris mitigation. We describe a method that contributes to achieving a requisite increase in orbit prediction accuracy for objects in the publicly available two-line element (TLE) catalog. Batch least-squares differential correction is applied to the TLEs. Using a high-precision numerical propagator, we fit an orbit to state vectors derived from successive TLEs. We then propagate the fitted orbit further forward in time. These predictions are validated against precision ephemeris data derived from the international laser ranging service (ILRS) for several satellites, including objects in the congested sun-synchronous orbital region. The method leads to a predicted range error that increases at a typical rate of 100 m per day, approximately a 10-fold improvement oyer individual TLE's propagated with their associated analytic propagator (SGP4). Corresponding improvements for debris trajectories could potentially provide conjunction analysis sufficiently accurate for an operationally viable collision avoidance system based on TLEs only.
We discuss additional optimization and the computational requirements for applying all-on-all conjunction analysis to the whole TLE catalog, present and near future. Finally, we outline a scheme for debris debris collision avoidance that may become practicable given these developments. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Levit, Creon; Marshall, William] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Marshall, William] Univ Space Res Assoc, Moffett Field, CA 94035 USA.
RP Levit, C (reprint author), NASA, Ames Res Ctr, MS202-3, Moffett Field, CA 94035 USA.
EM creon.levit@nasa.gov
NR 27
TC 14
Z9 23
U1 3
U2 20
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 APR 1
PY 2011
VL 47
IS 7
BP 1107
EP 1115
DI 10.1016/j.asr.2010.10.017
PG 9
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 741PS
UT WOS:000288876600001
ER
PT J
AU Yang, WW
Ponce, A
AF Yang, Wan-Wan
Ponce, Adrian
TI Validation of a Clostridium Endospore Viability Assay and Analysis of
Greenland Ices and Atacama Desert Soils
SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID GLACIER ICE; BACILLUS-SUBTILIS; BACTERIAL-SPORES; D-ALANINE;
MICROORGANISMS; GERMINATION; CORE; ENVIRONMENTS; LIFE; DECONTAMINATION
AB A microscopy-based endospore viability assay (micro-EVA) capable of enumerating germinable Clostridium endospores (GCEs) in less than 30 min has been validated and employed to determine GCE concentrations in Greenland ices and Atacama Desert soils. Inoculation onto agarose doped with Tb(3+) and D-alanine triggers Clostridium spore germination and the concomitant release of similar to 10(8) molecules of dipicolinic acid (DPA) per endospore, which, under pulsed UV excitation, enables enumeration of resultant green Tb(3+)-DPA luminescent spots as GCEs with time-gated luminescence microscopy. The intensity time courses of the luminescent spots were characteristic of stage I Clostridium spore germination dynamics. Micro-EVA was validated against traditional CFU cultivation from 0 to 1,000 total endospores/ml (i.e., phase-bright bodies/ml), yielding 56.4% +/- 1.5% GCEs and 43.0% +/- 1.0% CFU. We also show that D-alanine serves as a Clostridium-specific germinant (three species tested) that inhibits Bacillus germination of spores (five species tested) in that endospore concentration regime. Finally, GCE concentrations in Greenland ice cores and Atacama Desert soils were determined with micro-EVA, yielding 1 to 2 GCEs/ml of Greenland ice (versus <1 CFU/ml after 6 months of incubation) and 66 to 157 GCEs/g of Atacama Desert soil (versus 40 CFU/g soil).
C1 [Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ponce, A (reprint author), CALTECH, Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ponce@caltech.edu
FU DHS Science and Technology Directorate; NASA Astrobiology Institute;
Planetary Protection
FX We are grateful to the DHS Science and Technology Directorate, NASA
Astrobiology Institute, and Planetary Protection for funding.
NR 44
TC 8
Z9 8
U1 0
U2 5
PU AMER SOC MICROBIOLOGY
PI WASHINGTON
PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA
SN 0099-2240
J9 APPL ENVIRON MICROB
JI Appl. Environ. Microbiol.
PD APR
PY 2011
VL 77
IS 7
BP 2352
EP 2358
DI 10.1128/AEM.01966-10
PG 7
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA 741HT
UT WOS:000288855500020
PM 21296951
ER
PT J
AU Bonfils, X
Gillon, M
Forveille, T
Delfosse, X
Deming, D
Demory, BO
Lovis, C
Mayor, M
Neves, V
Perrier, C
Santos, NC
Seager, S
Udry, S
Boisse, I
Bonnefoy, M
AF Bonfils, X.
Gillon, M.
Forveille, T.
Delfosse, X.
Deming, D.
Demory, B. -O.
Lovis, C.
Mayor, M.
Neves, V.
Perrier, C.
Santos, N. C.
Seager, S.
Udry, S.
Boisse, I.
Bonnefoy, M.
TI A short-period super-Earth orbiting the M2.5 dwarf GJ 3634 Detection
with HARPS velocimetry and transit search with Spitzer photometry
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: radial velocities; stars: late-type; planetary systems
ID EXTRA-SOLAR PLANETS; LOW-MASS STARS; MAIN-SEQUENCE; DETECTABILITY;
METALLICITY; NEPTUNE; CATALOG
AB We report on the detection of GJ 3634b, a super-Earth of mass m sin i = 7.0(-0.8)(+0.9) M(circle plus) and period P = 2.64561 +/- 0.00066 day. Its host star is a M2.5 dwarf, has a mass of 0.45 +/- 0.05 M(circle dot), a radius of 0.43 +/- 0.03 R(circle dot) and lies 19.8 +/- 0.6 pc away from our Sun. The planet is detected after a radial-velocity campaign using the ESO/Harps spectrograph. GJ 3634b had an a priori geometric probability to undergo transit of similar to 7% and, if telluric in composition, a non-grazing transit would produce a photometric dip of less than or similar to 0.1%. We therefore followed-up upon the RV detection with photometric observations using the 4.5-mu m band of the IRAC imager onboard Spitzer. Our six-hour long light curve excludes that a transit occurs for 2 sigma of the probable transit window, decreasing the probability that GJ 3634b undergoes transit to similar to 0.5%.
C1 [Bonfils, X.; Forveille, T.; Delfosse, X.; Neves, V.; Perrier, C.; Bonnefoy, M.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France.
[Bonfils, X.; Gillon, M.; Lovis, C.; Mayor, M.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Gillon, M.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Deming, D.] NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA.
[Demory, B. -O.; Seager, S.] MIT, Dept Phys, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Neves, V.; Santos, N. C.; Boisse, I.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4150762 Oporto, Portugal.
RP Bonfils, X (reprint author), UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France.
EM Xavier.Bonfils@obs.ujf-grenoble.fr
RI Santos, Nuno/E-9957-2011;
OI Santos, Nuno/0000-0003-4422-2919; Bonfils, Xavier/0000-0001-9003-8894
FU European Research Council/European Community; Fundacao para a Ciencia e
a Tecnologia (FCT), Portugal [PTDC/CTE-AST/098528/2008,
PTDC/CTE-AST/098604/2008, SFRH/BD/60688/2009]; POPH/FSE (EC)
FX We thank the anonymous referee for his careful reading and suggestions.
M. G. is FNRS Research Associate. N.C.S., V.N. and I. B. acknowedge the
support by the European Research Council/European Community under the
FP7 through a Starting Grant, as well as in the form of grants reference
PTDC/CTE-AST/098528/2008, PTDC/CTE-AST/098604/2008 and
SFRH/BD/60688/2009, funded by Fundacao para a Ciencia e a Tecnologia
(FCT), Portugal. NCS would further like to thank the support from FCT
through a Ciencia 2007 contract funded by FCT/MCTES (Portugal) and
POPH/FSE (EC).
NR 40
TC 16
Z9 16
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A111
DI 10.1051/0004-6361/201015981
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600151
ER
PT J
AU Canuto, VM
AF Canuto, V. M.
TI Stellar mixing V. Overshooting
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE turbulence; diffusion; convection; hydrodynamics; methods: analytical;
stars: rotation
ID SOLAR CONVECTION ZONE; INTERNAL-ROTATION; MERIDIONAL FLOW; STARS;
TURBULENCE; EXTENT
AB Helio-seismological data suggest an overshooting (OV) extent of 0.07 H-p (H-p is the pressure scale height), while theoretical predictions from both models and numerical simulations yield values that are an order of magnitude higher. The reason identified by the authors of numerical simulations is the limited range of physical parameters allowed by the numerical simulations compared to the true solar values; specifically, the simulations are still too viscous. In the case of theoretical models, we discuss limitations that at present cannot be solved. For these reasons, we propose and work out a different methodology, which has in principle the following advantages. First, there is no longer a need to model the flux of turbulent kinetic energy, which has been a stumbling block for many years and whose modeling has introduced uncertainties that are difficult to control. Second, we account for processes not included before: shear (differential rotation), meridional currents, gravitational energy, stable-unstable stratification, and double diffusion.
C1 [Canuto, V. M.] Goddard Inst Space Studies, NASA, New York, NY 10025 USA.
[Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
RP Canuto, VM (reprint author), Goddard Inst Space Studies, NASA, New York, NY 10025 USA.
EM vmc13@columbia.edu
NR 24
TC 7
Z9 7
U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A80
DI 10.1051/0004-6361/201014450
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600024
ER
PT J
AU Canuto, VM
AF Canuto, V. M.
TI Stellar Mixing IV. The angular momentum problem
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE turbulence; diffusion; convection; hydrodynamics; methods: analytical;
stars: rotation
ID INTERNAL GRAVITY-WAVES; REYNOLDS STRESS MODEL; LOW-MASS STARS; TURBULENT
CONVECTION; DIFFERENTIAL ROTATION; SOLAR INTERIOR; MAIN-SEQUENCE;
TRANSPORT; FORMALISM; FLOWS
AB We present a formalism that provides the Reynolds stresses needed to solve the angular momentum equation. The traditional Reynolds stress model assumes that the only contribution comes from shear (a down-gradient flux), but this leads to an extraction of angular momentum from the interior that is far too small compared to what is required to explain the helio seismological data. An illustrative solution of the new Reynolds stress equations shows that the presence of vorticity in a stably stratified regime, such as the one in the radiative zone, contributes a new term to the angular momentum equation that has an up-gradient flux like the one provided by the IGW model (internal gravity waves). The time scale entailed by such a term may be of the same order of 10(7) yrs produced by the IGW model. It would be instructive to solve the new angular momentum equation together with the formalism developed in Paper III to study not only the solar angular momentum distribution vs. helio data, but also the evolution of elements such as (7)Li and (4)He. These results would allow a more quantitative assessment of the overall model.
The complete model yields Reynolds stresses that include differential rotation, unstable/stable stratification, double diffusion, radiative losses (arbitrary Peclet number), and meridional currents.
C1 [Canuto, V. M.] Goddard Inst Space Studies, NASA, New York, NY 10025 USA.
[Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
RP Canuto, VM (reprint author), Goddard Inst Space Studies, NASA, New York, NY 10025 USA.
EM vmc13@columbia.edu
NR 28
TC 5
Z9 5
U1 0
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A79
DI 10.1051/0004-6361/201014449
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600023
ER
PT J
AU Canuto, VM
AF Canuto, V. M.
TI Stellar mixing III. The case of a passive tracer
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE diffusion; instabilities; turbulence; stars: interiors; convection;
methods: analytical
ID DIFFUSION-PROCESSES; RELEASE EXPERIMENT; SALT FINGERS; STARS;
PYCNOCLINE; TURBULENCE; ROTATION
AB In Papers I-II, we derived the expressions for the turbulent diffusivities of momentum, temperature T, and mean molecular weight mu. Since the scalar T-mu fields are active tracers (by influencing the density and thus the velocity field), whereas passive tracers such as(7)Li are carried along by the flow without influencing it, it would be unjustified to use the diffusivities of the T-mu fields to represent the diffusivity of passive tracers.
In this paper, we present the first derivation of a passive tracer diffusivity. Some key results are:
a) In the general 3D case, the passive tracer diffusivity is a tensor given in algebraic form; b) the diffusivity tensor depends on shear, vorticity, T, and mu-gradients, thus including double diffusion and differential rotation; c) in the 1D version of the model, the passive tracer diffusivity is a scalar denoted by K-c; d) in doubly stable regimes, del(mu) > 0, del - del(ad) < 0, K-c is nearly the same as those of the T-mu fields; e) in semi-convection regimes, del(mu) > 0, del - del(ad) > 0, K-c is larger than that of the mu-field; f) in salt fingers regimes del(mu) < 0, del - del(ad) < 0, K-c is smaller than that of the mu-field; and finally, g) in the only case we know of a direct measurement of a passive tracer diffusivity, the oceanographic North Atlantic Tracer Release Experiment (NATRE), the model reproduces the data quite closely.
C1 [Canuto, V. M.] Goddard Inst Space Studies, NASA, New York, NY 10025 USA.
[Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
RP Canuto, VM (reprint author), Goddard Inst Space Studies, NASA, New York, NY 10025 USA.
EM vmc13@columbia.edu
NR 16
TC 4
Z9 4
U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A78
DI 10.1051/0004-6361/201015372
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600022
ER
PT J
AU Canuto, VM
AF Canuto, V. M.
TI Stellar mixing I. Formalism
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE turbulence; diffusion; convection; hydrodynamics; methods: analytical;
stars: rotation
ID TURBULENCE CLOSURE-MODEL; STABLY STRATIFIED FLOWS; LOW-MASS STARS;
BOUNDARY-LAYER; DIFFERENTIAL ROTATION; RICHARDSON-NUMBER; SURFACE;
CONVECTION; HEAT; STABILITY
AB In this paper we use the Reynolds stress models (RSM) to derive algebraic expressions for the following variables: a) heat fluxes; b) mu fluxes; and c) momentum fluxes. These relations, which are fully 3D, include:
1) stable and unstable stratification, represented by the Brunt-Vaisala frequency, N-2 = -gH(p)(-1)(del - del(ad))(1 - R-mu);
2) double diffusion, salt-fingers, and semi-convection, represented by the density ratio R-mu = del(mu)(del - del(ad))(-1);
3) shear (differential rotation), represented by the mean squared shear Sigma(2) or by the Richardson number, Ri = N-2 Sigma(-2);
4) radiative losses represented by a Peclet number, Pe;
5) a complete analytical solution of the 1D version of the model. In general, the model requires the solution of two differential equations for the eddy kinetic energy K and its rate of dissipation, e. In the local and stationary cases, when production equals dissipation, the model equations are all algebraic.
C1 [Canuto, V. M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
RP Canuto, VM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM vmc13@columbia.edu
NR 48
TC 14
Z9 14
U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A76
DI 10.1051/0004-6361/201014447
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600020
ER
PT J
AU Canuto, VM
AF Canuto, V. M.
TI Stellar mixing II. Double diffusion processes
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE turbulence; diffusion; convection; hydrodynamics; methods: analytical;
stars: rotation
ID LOW-MASS STARS; THERMOHALINE CONVECTION; RGB-STARS; ROTATION; BLUE;
PYCNOCLINE; TURBULENCE; SEQUENCE; FINGERS; TRACER
AB In this paper, salt-fingers (also called thermohaline convection) and semi-convection are treated under the name of double-diffusion (DD). We present and discuss the solutions of the RSM(Reynolds stress models) equations that provide the momentum, heat, mu fluxes, and their corresponding diffusivities denoted by K-m,K-h,K-mu. Such fluxes are given by a set of linear, algebraic equations that depend on the following variables: mean velocity gradient (differential rotation), temperature gradients (for both stable and unstable regimes), and mu-gradients (DD). Some key results are as follows. Salt-fingers. When shear is strong and DD is inefficient, heat and mu diffusivities are identical. Second, when shear is weak K-mu > K-h and the difference can be sizeable O(10) meaning that heat and mu diffusivities must therefore be treated as different. Third, for strong-to-moderate shears and for R-mu less than 0.8, both heat and mu diffusivities are practically independent of R-mu. Fourth, the latter result favors parameterizations of the type K-h,K-mu similar to CR mu 0 suggested by some authors. Our results, however, show that C is not a constant but a linear function of the Reynolds number Re = epsilon(nu N-2)(-1) defined in terms of the kinematic viscosity nu, the Brunt-Vaisala frequency N, and the rate of energy input into the system, epsilon. Fifth, we suggest that epsilon is an essential ingredient that has been missing in all diffusivity models, but which ought to be present because without a source of energy, turbulence dies out and so does the turbulent mixing (for example, the turbulent kinetic energy is proportional to the power 2/3 of epsilon). Moreover, since different stellar environments have different epsilon, its presence is necessary for differentiating mixing regimes in different stars. Semi-convection. In this case the destabilizing effect is the T-gradient, and when shear is weak, K-h > K-mu. Since the model is symmetric under the change R-mu to R-mu(-1), most of the results obtained in the previous case can be translated to this case.
C1 [Canuto, V. M.] Goddard Inst Space Studies, NASA, New York, NY 10025 USA.
[Canuto, V. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
RP Canuto, VM (reprint author), Goddard Inst Space Studies, NASA, New York, NY 10025 USA.
EM vmc13@columbia.edu
NR 27
TC 8
Z9 8
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A77
DI 10.1051/0004-6361/201014448
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600021
ER
PT J
AU Giroletti, M
Paragi, Z
Bignall, H
Doi, A
Foschini, L
Gabanyi, KE
Reynolds, C
Blanchard, J
Campbell, RM
Colomer, F
Hong, X
Kadler, M
Kino, M
van Langevelde, HJ
Nagai, H
Phillips, C
Sekido, M
Szomoru, A
Tzioumis, AK
AF Giroletti, M.
Paragi, Z.
Bignall, H.
Doi, A.
Foschini, L.
Gabanyi, K. E.
Reynolds, C.
Blanchard, J.
Campbell, R. M.
Colomer, F.
Hong, X.
Kadler, M.
Kino, M.
van Langevelde, H. J.
Nagai, H.
Phillips, C.
Sekido, M.
Szomoru, A.
Tzioumis, A. K.
TI Global e-VLBI observations of the gamma-ray narrow line Seyfert 1 PMN
J0948+0022
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; galaxies: jets; instrumentation:
high angular resolution; instrumentation: interferometers
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; RADIO-LOUD; RELATIVISTIC
JET; QUASAR; EMISSION; DISCOVERY; GALAXIES
AB Context. There is growing evidence of relativistic jets in radio-loud narrow-line Seyfert 1 (RL-NLS1) galaxies.
Aims. We constrain the observational properties of the radio emission in the first RL-NLS1 galaxy ever detected in gamma-rays, PMN J0948+0022, i.e., its flux density and structure in both total intensity and polarization, its compactness, and variability.
Methods. We performed three real-time e-VLBI observations of PMN J0948+0022 at 22 GHz, using a global array including telescopes in Europe, East Asia, and Australia. These are the first e-VLBI science observations ever carried out with a global array, reaching a maximum baseline length of 12 458 km. The observations were part of a large multiwavelength campaign in 2009.
Results. The source is detected at all three epochs. The structure is dominated by a bright component, more compact than 55 mu as, with a fainter component at a position angle theta similar to 35 degrees. Relativistic beaming is required by the observed brightness temperature of 3.4 x 10(11) K. Polarization is detected at a level of about 1%.
Conclusions. The parameters derived by the VLBI observations, in addition to the broad-band properties, confirm that PMN J0948+0022 is similar to flat spectrum radio quasars. Global e-VLBI is a reliable and promising technique for future studies.
C1 [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Paragi, Z.; Campbell, R. M.; van Langevelde, H. J.; Szomoru, A.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands.
[Paragi, Z.; Gabanyi, K. E.] MTA Res Grp Phys Geodesy & Geodynam, H-1521 Budapest, Hungary.
[Bignall, H.; Reynolds, C.] Curtin Univ, ICRAR Curtin Inst Radio Astron, Perth, WA 6845, Australia.
[Doi, A.; Nagai, H.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Foschini, L.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Gabanyi, K. E.] FOMI Satellite Geodet Observ, H-1592 Budapest, Hungary.
[Blanchard, J.] Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia.
[Colomer, F.] Observ Astron Nacl, Madrid 28014, Spain.
[Hong, X.] Shanghai Astron Observ, Shanghai 200030, Peoples R China.
[Kadler, M.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
[Kadler, M.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Kino, M.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[van Langevelde, H. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Phillips, C.; Tzioumis, A. K.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Sekido, M.] NIICT, Kashima Space Res Ctr, Kashima, Ibaraki 314, Japan.
RP Giroletti, M (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
EM giroletti@ira.inaf.it
RI Foschini, Luigi/H-3833-2012; Reynolds, Cormac/B-5635-2013; Bignall,
Hayley/B-2867-2013;
OI van Langevelde, Huib Jan/0000-0002-0230-5946; Foschini,
Luigi/0000-0001-8678-0324; Reynolds, Cormac/0000-0002-8978-0626;
Bignall, Hayley/0000-0001-6247-3071; Giroletti,
Marcello/0000-0002-8657-8852; Kadler, Matthias/0000-0001-5606-6154
FU European Community [227290]; Italian Ministry of Foreign Affairs, Japan;
Italian Ministry of Foreign Affairs, Italy; Communication Network
Developments project "EXPReS" [02662]; Commonwealth of Australia
FX The authors are grateful to Richard Dodson and Daniele Dallacasa for
useful discussions on the polarization calibration, and to Uwe Bach for
providing calibration data from the 100-m telescope of the MPIfR
(Max-Planck-Institut fur Radioastronomie) at Effelsberg. This activity
is supported by the European Community Framework Programme 7, Advanced
Radio Astronomy in Europe, grant agreement No. 227290 and by the Italian
Ministry of Foreign Affairs within the Scientific and Technology
Cooperation Agreement between Japan and Italy. e-VLBI developments in
Europe are supported by the EC DG-INFSO funded Communication Network
Developments project "EXPReS", Contract No. 02662
(http://www.expres-eu.org/). The European VLBI Network
(http://www.evlbi.org/) is a joint facility of European, Chinese, South
African and other radio astronomy institutes funded by their national
research councils. The Long Baseline Array is part of the Australia
Telescope National Facility which is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO.
NR 27
TC 22
Z9 22
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR L11
DI 10.1051/0004-6361/201116639
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600011
ER
PT J
AU Gruber, D
Kruhler, T
Foley, S
Nardini, M
Burlon, D
Rau, A
Bissaldi, E
von Kienlin, A
McBreen, S
Greiner, J
Bhat, PN
Briggs, MS
Burgess, JM
Chaplin, VL
Connaughton, V
Diehl, R
Fishman, GJ
Gibby, MH
Giles, MM
Goldstein, A
Guiriec, S
van der Horst, AJ
Kippen, RM
Kouveliotou, C
Lin, L
Meegan, CA
Paciesas, WS
Preece, RD
Tierney, D
Wilson-Hodge, C
AF Gruber, D.
Kruehler, T.
Foley, S.
Nardini, M.
Burlon, D.
Rau, A.
Bissaldi, E.
von Kienlin, A.
McBreen, S.
Greiner, J.
Bhat, P. N.
Briggs, M. S.
Burgess, J. M.
Chaplin, V. L.
Connaughton, V.
Diehl, R.
Fishman, G. J.
Gibby, M. H.
Giles, M. M.
Goldstein, A.
Guiriec, S.
van der Horst, A. J.
Kippen, R. M.
Kouveliotou, C.
Lin, L.
Meegan, C. A.
Paciesas, W. S.
Preece, R. D.
Tierney, D.
Wilson-Hodge, C.
TI Fermi/GBM observations of the ultra-long GRB 091024 A burst with an
optical flash
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst: individual: GRB 091024
ID GAMMA-RAY-BURSTS; PROBE WMAP OBSERVATIONS; LAG-LUMINOSITY RELATION;
LIGHT CURVES; PEAK LUMINOSITY; COSMOLOGICAL PARAMETERS; SPECTRAL
EVOLUTION; BATSE OBSERVATIONS; AFTERGLOW; BRIGHT
AB Aims. In this paper we examine gamma-ray and optical data of GRB 091024, a gamma-ray burst (GRB) with an extremely long duration of T-90 approximate to 1020 s, as observed with the Fermi Gamma-ray Burst Monitor (GBM).
Methods. We present spectral analysis of all three distinct emission episodes using data from Fermi/GBM. Because of the long nature of this event, many ground-based optical telescopes slewed to its location within a few minutes and thus were able to observe the GRB during its active period. We compare the optical and gamma-ray light curves. Furthermore, we estimate a lower limit on the bulk Lorentz factor from the variability and spectrum of the GBM light curve and compare it with that obtained from the peak time of the forward shock of the optical afterglow.
Results. From the spectral analysis we note that, despite its unusually long duration, this burst is similar to other long GRBs, i.e. there is spectral evolution (both the peak energy and the spectral index vary with time) and spectral lags are measured. We find that the optical light curve is highly anti-correlated to the prompt gamma-ray emission, with the optical emission reaching the maximum during an epoch of quiescence in the prompt emission. We interpret this behavior as the reverse shock (optical flash), expected in the internal-external shock model of GRB emission but observed only in a handful of GRBs so far. The lower limit on the initial Lorentz factor deduced from the variability time scale (Gamma(min) = 195(-110)(+ 90)) is consistent within the error to the one obtained using the peak time of the forward shock (Gamma(0) = 120) and is also consistent with Lorentz factors of other long GRBs.
C1 [Gruber, D.; Kruehler, T.; Foley, S.; Nardini, M.; Burlon, D.; Rau, A.; Bissaldi, E.; von Kienlin, A.; Greiner, J.; Diehl, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany.
[McBreen, S.; Tierney, D.] Univ Coll Dublin, Dublin 4, Ireland.
[Bhat, P. N.; Briggs, M. S.; Burgess, J. M.; Chaplin, V. L.; Connaughton, V.; Goldstein, A.; Guiriec, S.; van der Horst, A. J.; Paciesas, W. S.; Preece, R. D.] Univ Alabama, NSSTC, Huntsville, AL 35805 USA.
[Fishman, G. J.; Kouveliotou, C.; Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Gibby, M. H.; Giles, M. M.] Jacobs Technol Inc, Huntsville, AL USA.
[Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Meegan, C. A.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA.
RP Gruber, D (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr,Postfach 1312, D-85748 Garching, Germany.
EM dgruber@mpe.mpg.de
RI Bissaldi, Elisabetta/K-7911-2016;
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece,
Robert/0000-0003-1626-7335; Burgess, James/0000-0003-3345-9515;
Kruehler, Thomas/0000-0002-8682-2384
FU German Bundesministerium fur Wirtschaft und Technologie (BMWi) via the
Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50 QV 0301, 50 OG
0502]; Irish Research Council for Science, Engineering and Technology;
Marie Curie Actions
FX The GBM project is supported by the German Bundesministerium fur
Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft-
und Raumfahrt (DLR) under the contract numbers 50 QV 0301 and 50 OG
0502. S.F. acknowledges the support of the Irish Research Council for
Science, Engineering and Technology, cofunded by Marie Curie Actions
under FP7.
NR 65
TC 25
Z9 25
U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A15
DI 10.1051/0004-6361/201015891
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600041
ER
PT J
AU Liuzzo, E
Falomo, R
Treves, A
Donato, D
Sambruna, M
Arcidiacono, C
Giovannini, G
Farinato, J
Moretti, A
Ragazzoni, R
Diolaiti, E
Lombini, M
Brast, R
Donaldson, R
Kolb, J
Marchetti, E
Tordo, S
AF Liuzzo, E.
Falomo, R.
Treves, A.
Donato, D.
Sambruna, M.
Arcidiacono, C.
Giovannini, G.
Farinato, J.
Moretti, A.
Ragazzoni, R.
Diolaiti, E.
Lombini, M.
Brast, R.
Donaldson, R.
Kolb, J.
Marchetti, E.
Tordo, S.
TI The jet of the BL Lacertae object PKS 2201+044: MAD near-IR adaptive
optics observations and comparison with optical, radio and X-ray data
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE BL Lacertae objects: individual: PKS 2201+044; instrumentation: adaptive
optics
ID HUBBLE-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; M87 JET; HOST GALAXIES;
EMISSION; CHANDRA; 3C-273; VARIABILITY; CANDIDATES; MORPHOLOGY
AB Context. Relativistic jets are a common feature of radio loud active galactic nuclei. Multifrequency observations are a unique tool to constrain their physics.
Aims. We report on a detailed study of the properties of the jet of the nearby BL Lac object PKS 2201+044, one of the rare cases where the jet is detected from radio to X-rays.
Methods. We use new adaptive optics near-IR observations of the source, obtained with the ESO multi-conjugated adaptive optics demonstrator (MAD) at the Very Large Telescope. These observations acquired in Ground-Layer Adaptive Optics mode are combined with images previously achieved by HST, VLA and Chandra to perform a morphological and photometric study of the jet.
Results. We find a noticeable similarity in the morphology of the jet at radio, near-IR and optical wavelengths. We construct the spectral shape of the main knot of jet that appears dominated by synchrotron radiation.
Conclusions. On the basis of the jet morphology and the weak lines spectrum we suggest that PKS 2201+044 belongs to the class of radio sources intermediate between FRIs and FRIIs.
C1 [Liuzzo, E.; Giovannini, G.; Brast, R.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[Liuzzo, E.; Giovannini, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Falomo, R.; Arcidiacono, C.; Farinato, J.; Moretti, A.; Ragazzoni, R.] INAF, Osservatorio Astron Padova, I-35122 Padua, Italy.
[Treves, A.] Univ Insubria Como, INAF, Varese, Italy.
[Treves, A.] Ist Nazl Fis Nucl, Milan, Italy.
[Donato, D.; Sambruna, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lombini, M.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Donaldson, R.; Kolb, J.; Marchetti, E.; Tordo, S.] European So Observ, D-85748 Garching, Germany.
RP Liuzzo, E (reprint author), INAF, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
EM liuzzo@ira.inaf.it
RI Moretti, Alessia/I-8361-2012;
OI Farinato, Jacopo/0000-0002-5840-8362; Giovannini,
Gabriele/0000-0003-4916-6362; lombini, matteo/0000-0002-5920-2139;
Ragazzoni, Roberto/0000-0002-7697-5555; Falomo,
Renato/0000-0003-4137-6541; Arcidiacono, Carmelo/0000-0003-0142-8108;
Moretti, Alessia/0000-0002-1688-482X
FU European Union; Valle D'Aosta Region; Italian Minister; National
Aeronautics and Space Administration
FX We wish to thank Teddy Cheung for his work on radio data reduction. This
work was supported by contributions of European Union, Valle D'Aosta
Region and the Italian Minister for Work and Welfare. This research has
made use of the NASA/IPAC Extragalactic Data Base (NED), which is
operated by the JPL, California Institute of Technology, under contract
with the National Aeronautics and Space Administration.
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A34
DI 10.1051/0004-6361/201015570
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600046
ER
PT J
AU Puccetti, S
Capalbi, M
Giommi, P
Perri, M
Stratta, G
Angelini, L
Burrows, DN
Campana, S
Chincarini, G
Cusumano, G
Gehrels, N
Moretti, A
Nousek, J
Osborne, JP
Tagliaferri, G
AF Puccetti, S.
Capalbi, M.
Giommi, P.
Perri, M.
Stratta, G.
Angelini, L.
Burrows, D. N.
Campana, S.
Chincarini, G.
Cusumano, G.
Gehrels, N.
Moretti, A.
Nousek, J.
Osborne, J. P.
Tagliaferri, G.
TI The Swift serendipitous survey in deep XRT GRB fields (SwiftFT) I. The
X-ray catalog and number counts
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: general; surveys; catalogs; galaxies: active
ID N-LOG S; CHANDRA MULTIWAVELENGTH PROJECT; POINT-SOURCE CATALOGS; MS
SOURCE CATALOGS; LOCKMAN-HOLE; COSMOS FIELD; HELLAS2XMM SURVEY; NORTH
SURVEY; SOUTH SURVEY; EVOLUTION
AB Aims. An accurate census of the active galactic nuclei (AGN) is a key step in investigating the nature of the correlation between the growth and evolution of super massive black holes and galaxy evolution. X-ray surveys provide one of the most efficient ways of selecting AGN.
Methods. We searched for X-ray serendipitous sources in over 370 Swift-XRT fields centered on gamma ray bursts detected between 2004 and 2008 and observed with total exposures ranging from 10 ks to over 1 Ms. This defines the Swift Serendipitous Survey in deep XRT GRB fields, which is quite broad compared to existing surveys (similar to 33 square degrees) and medium depth, with a faintest flux limit of 7.2 x 10(-16) erg cm(-2) s(-1) in the 0.5 to 2 keV energy range (4.8 x 10(-15) erg cm(-2) s(-1) at 50% completeness). The survey has a high degree of uniformity thanks to the stable point spread function and small vignetting correction factors of the XRT, moreover is completely random on the sky as GRBs explode in totally unrelated parts of the sky.
Results. In this paper we present the sample and the X-ray number counts of the high Galactic-latitude sample, estimated with high statistics over a wide flux range (i.e., 7.2x10(-1)6 divided by similar to 5x10(-13) erg cm(-2) s(-1) in the 0.5-2 keV band and 3.4x10(-15)similar to divided by 6x10(-13) erg cm(-2) s(-1) in the 2-10 keV band). We detect 9387 point-like sources with a detection Poisson probability threshold of <= 2x10(-5), in at least one of the three energy bands considered (i.e. 0.3-3 keV, 2-10 keV, and 0.3-10 keV), for the total sample, while 7071 point-like sources are found at high Galactic-latitudes (i.e. |b|>= 20 deg). The large number of detected sources resulting from the combination of large area and deep flux limits make this survey a new important tool for investigating the evolution of AGN. In particular, the large area permits finding rare high-luminosity objects like QSO2, which are poorly sampled by other surveys, adding precious information for the luminosity function bright end. The high Galactic-latitude log N-log S relation is well determined over all the flux coverage, and it is nicely consistent with previous results at 1 sigma confidence level. By the hard X-ray color analysis, we find that the Swift Serendipitous Survey in deep XRT GRB fields samples relatively unobscured and mildly obscured AGN, with a fraction of obscured sources of similar to 37% (similar to 15%) in the 2-10 (0.3-3 keV) band.
C1 [Puccetti, S.; Capalbi, M.; Giommi, P.; Perri, M.; Stratta, G.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Angelini, L.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burrows, D. N.; Nousek, J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Campana, S.; Chincarini, G.; Moretti, A.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy.
[Chincarini, G.] Univ Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy.
[Cusumano, G.] Ist Astrofis Spaziale & Fis Cosm Palermo, INAF, I-90146 Palermo, Italy.
[Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Puccetti, S (reprint author), ASI Sci Data Ctr, Via Galileo Galilei, I-00044 Frascati, Italy.
EM puccetti@asdc.asi.it
RI Gehrels, Neil/D-2971-2012; Stratta, Maria Giuliana/L-3045-2016;
OI Stratta, Maria Giuliana/0000-0003-1055-7980; Campana,
Sergio/0000-0001-6278-1576; giommi, paolo/0000-0002-2265-5003; Cusumano,
Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315;
Puccetti, Simonetta/0000-0002-2734-7835; Perri,
Matteo/0000-0003-3613-4409; Tagliaferri, Gianpiero/0000-0003-0121-0723
FU STFC
FX S.P. acknowledges F. Fiore for the useful discussions. J.P.O.
acknowledges the support of the STFC. We acknowledge the anonymous
referee for his comments, that helped improving the quality of the
manuscript.
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PI LES ULIS CEDEX A
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FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
AR A122
DI 10.1051/0004-6361/201015560
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600167
ER
PT J
AU Ricci, D
Poels, J
Elyiv, A
Finet, F
Sprimont, PG
Anguita, T
Bozza, V
Browne, P
Burgdorf, M
Novati, SC
Dominik, M
Dreizler, S
Glitrup, M
Grundahl, F
Harpsoe, K
Hessman, F
Hinse, TC
Hornstrup, A
Hundertmark, M
Jorgensen, UG
Liebig, C
Maier, G
Mancini, L
Masi, G
Mathiasen, M
Rahvar, S
Scarpetta, G
Skottfelt, J
Snodgrass, C
Southworth, J
Teuber, J
Thone, CC
Wambsganss, J
Zimmer, F
Zub, M
Surdej, J
AF Ricci, D.
Poels, J.
Elyiv, A.
Finet, F.
Sprimont, P. G.
Anguita, T.
Bozza, V.
Browne, P.
Burgdorf, M.
Novati, S. Calchi
Dominik, M.
Dreizler, S.
Glitrup, M.
Grundahl, F.
Harpsoe, K.
Hessman, F.
Hinse, T. C.
Hornstrup, A.
Hundertmark, M.
Jorgensen, U. G.
Liebig, C.
Maier, G.
Mancini, L.
Masi, G.
Mathiasen, M.
Rahvar, S.
Scarpetta, G.
Skottfelt, J.
Snodgrass, C.
Southworth, J.
Teuber, J.
Thone, C. C.
Wambsganss, J.
Zimmer, F.
Zub, M.
Surdej, J.
TI Flux and color variations of the quadruply imaged quasar HE 0435-1223
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE quasars: general; gravitational lensing: weak; techniques: photometric
ID GRAVITATIONAL LENS; TIME-DELAY; GALAXY; QSO; HE-0435-1223; VARIABILITY;
Q2237+0305
AB Aims. We present VRi photometric observations of the quadruply imaged quasar HE0435-1223, carried out with the Danish 1.54 m telescope at the La Silla Observatory. Our aim was to monitor and study the magnitudes and colors of each lensed component as a function of time.
Methods. We monitored the object during two seasons (2008 and 2009) in the VRi spectral bands, and reduced the data with two independent techniques: difference imaging and point spread function (PSF) fitting.
Results. Between these two seasons, our results show an evident decrease in flux by approximate to 0.2-0.4 magnitudes of the four lensed components in the three filters. We also found a significant increase (approximate to 0.05-0.015) in their V - R and R - i color indices.
Conclusions. These flux and color variations are very likely caused by intrinsic variations of the quasar between the observed epochs. Microlensing effects probably also affect the brightest "A" lensed component.
C1 [Ricci, D.; Poels, J.; Elyiv, A.; Finet, F.; Sprimont, P. G.; Surdej, J.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege 1, Belgium.
[Elyiv, A.] Ukrainian Acad Sci, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Anguita, T.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Ctr Astro Ingn, Santiago, Chile.
[Anguita, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84085 Fisciano, SA, Italy.
[Bozza, V.; Scarpetta, G.] Inst Nazl Fis Nucl, Sez Napoli, Milan, Italy.
[Browne, P.; Dominik, M.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Burgdorf, M.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Novati, S. Calchi; Mancini, L.] IIASS, Vietri Sul Mare, SA, Italy.
[Dreizler, S.; Hessman, F.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Harpsoe, K.; Hinse, T. C.; Jorgensen, U. G.; Mathiasen, M.; Skottfelt, J.; Teuber, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Hinse, T. C.] KASI Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Hornstrup, A.] Tech Univ Denmark, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Liebig, C.; Maier, G.; Wambsganss, J.; Zimmer, F.; Zub, M.] Univ Heidelberg, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany.
[Mancini, L.] Univ Sannio, Dipartimento Ingn, I-82100 Benevento, Italy.
[Masi, G.] Ctr Backyard Astrophys, Bellatrix Astron Observ, Ceccano, FR, Italy.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Snodgrass, C.] European So Observ, Santiago 19, Chile.
[Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Southworth, J.] Univ Keele, Astrophys Grp, Newcastle Under Lyme ST5 5BG, England.
[Thone, C. C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Thone, C. C.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy.
[Burgdorf, M.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Harpsoe, K.; Jorgensen, U. G.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
RP Ricci, D (reprint author), Univ Liege, Dept Astrophys Geophys & Oceanog, Bat B5C, B-4000 Liege 1, Belgium.
EM ricci@astro.ulg.ac.be
RI Zimmer, Fabian/M-4765-2014; Hundertmark, Markus/C-6190-2015; Rahvar,
Sohrab/A-9350-2008;
OI Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Thone,
Christina/0000-0002-7978-7648; Ricci, Davide/0000-0002-9790-0552;
Snodgrass, Colin/0000-0001-9328-2905
FU ARC - Action de recherche concertee (Communaute Francaise de Belgique -
Academie Wallonie-Europe); Belgian Federal Science Policy Office;
Department of Culture, Arts & Leisure (DCAL), Northern Ireland, UK
FX The research was supported by ARC - Action de recherche concertee
(Communaute Francaise de Belgique - Academie Wallonie-Europe). A.E. is
the beneficiary of a fellowship granted by the Belgian Federal Science
Policy Office. Astronomical research at Armagh Observatory is funded by
the Department of Culture, Arts & Leisure (DCAL), Northern Ireland, UK.
Operation of the Danish 1.54 m telescope is supported by the Danish
National Science Research Council (FNU). We wish to thank the anonymous
referee for the remarks and the suggestions.
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2011
VL 528
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DI 10.1051/0004-6361/201016188
PG 8
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SC Astronomy & Astrophysics
GA 737BD
UT WOS:000288541600048
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Antolini, E
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bonamente, E
Borgland, AW
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Cannon, A
Caraveo, PA
Carrigan, S
Casandjian, JM
Cecchi, C
Celik, O
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Costamante, L
Cutini, S
Dermer, CD
de Palma, F
Donato, D
Silva, EDE
Drell, PS
Dubois, R
Escande, L
Favuzzi, C
Fegan, SJ
Finke, J
Focke, WB
Fortin, P
Frailis, M
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guiriec, S
Hadasch, D
Hayashida, M
Hays, E
Hughes, RE
Itoh, R
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Lee, SH
Garde, ML
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Makeev, A
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Naumann-Godo, M
Nishino, S
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Ritz, S
Roth, M
Sadrozinski, HFW
Sanchez, D
Sander, A
Schinzel, FK
Sgro, C
Siskind, EJ
Smith, PD
Sokolovsky, KV
Spandre, G
Spinelli, P
Strickman, MS
Suson, DJ
Takahashi, H
Tanaka, T
Thayer, JB
Thayer, JG
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Tramacere, A
Uehara, T
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vilchez, N
Vitale, V
Waite, AP
Wallace, E
Wang, P
Winer, BL
Wood, KS
Yang, Z
Ylinen, T
Ziegler, M
Berdyugin, A
Boettcher, M
Carraminana, A
Carrasco, L
de la Fuente, E
Diltz, C
Hovatta, T
Kadenius, V
Kovalev, YY
Lahteenmaki, A
Lindfors, E
Marscher, AP
Nilsson, K
Pereira, D
Reinthal, R
Roustazadeh, P
Savolainen, T
Sillanpaa, A
Takalo, LO
Tornikoski, M
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Antolini, E.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Cannon, A.
Caraveo, P. A.
Carrigan, S.
Casandjian, J. M.
Cecchi, C.
Celik, Oe
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Costamante, L.
Cutini, S.
Dermer, C. D.
de Palma, F.
Donato, D.
do Couto e Silva, E.
Drell, P. S.
Dubois, R.
Escande, L.
Favuzzi, C.
Fegan, S. J.
Finke, J.
Focke, W. B.
Fortin, P.
Frailis, M.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guiriec, S.
Hadasch, D.
Hayashida, M.
Hays, E.
Hughes, R. E.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Lee, S. -H.
Garde, M. Llena
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Makeev, A.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Naumann-Godo, M.
Nishino, S.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Ritz, S.
Roth, M.
Sadrozinski, H. F. -W.
Sanchez, D.
Sander, A.
Schinzel, F. K.
Sgro, C.
Siskind, E. J.
Smith, P. D.
Sokolovsky, K. V.
Spandre, G.
Spinelli, P.
Strickman, M. S.
Suson, D. J.
Takahashi, H.
Tanaka, T.
Thayer, J. B.
Thayer, J. G.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Tramacere, A.
Uehara, T.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vilchez, N.
Vitale, V.
Waite, A. P.
Wallace, E.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Ylinen, T.
Ziegler, M.
Berdyugin, A.
Boettcher, M.
Carraminana, A.
Carrasco, L.
de la Fuente, E.
Diltz, C.
Hovatta, T.
Kadenius, V.
Kovalev, Y. Y.
Lahteenmaki, A.
Lindfors, E.
Marscher, A. P.
Nilsson, K.
Pereira, D.
Reinthal, R.
Roustazadeh, P.
Savolainen, T.
Sillanpaa, A.
Takalo, L. O.
Tornikoski, M.
TI THE FIRST FERMI MULTIFREQUENCY CAMPAIGN ON BL LACERTAE: CHARACTERIZING
THE LOW-ACTIVITY STATE OF THE EPONYMOUS BLAZAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; BL Lacertae objects: individual (BL
Lacertae); galaxies: jets; gamma rays: galaxies; radiation mechanisms:
non-thermal; X-rays: galaxies
ID LARGE-AREA TELESCOPE; RAY LIGHT CURVES; GAMMA-RAY; MULTIWAVELENGTH
OBSERVATIONS; SPECTRAL VARIABILITY; GALACTIC NUCLEI; WEBT CAMPAIGNS;
1997 OUTBURST; OCTOBER 2007; EGRET DATA
AB We report on observations of BL Lacertae during the first 18 months of Fermi LAT science operations and present results from a 48 day multifrequency coordinated campaign from 2008 August 19 to 2008 October 7. The radio to gamma-ray behavior of BL Lac is unveiled during a low-activity state thanks to the coordinated observations of radio-band (Metsahovi and VLBA), near-IR/optical (Tuorla, Steward, OAGH, and MDM), and X-ray (RXTE and Swift) observatories. No variability was resolved in gamma rays during the campaign, and the brightness level was 15 times lower than the level of the 1997 EGRET outburst. Moderate and uncorrelated variability has been detected in UV and X-rays. The X-ray spectrum is found to be concave, indicating the transition region between the low- and high-energy components of the spectral energy distribution (SED). VLBA observation detected a synchrotron spectrum self-absorption turnover in the innermost part of the radio jet appearing to be elongated and inhomogeneous, and constrained the average magnetic field there to be less than 3 G. Over the following months, BL Lac appeared variable in gamma rays, showing flares (in 2009 April and 2010 January). There is no evidence for the correlation of gamma rays with the optical flux monitored from the ground in 18 months. The SED may be described by a single-zone or a two-zone synchrotron self-Compton (SSC) model, but a hybrid SSC plus external radiation Compton model seems to be preferred based on the observed variability and the fact that it provides a fit closest to equipartition.
C1 [Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Finke, J.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Abdo, A. A.; Cheung, C. C.; Finke, J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Tibaldo, L.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[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.; Fortin, P.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Cannon, A.; Celik, Oe; Gehrels, N.; Hays, E.; McEnery, J. E.; Thompson, D. J.; Pereira, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cannon, A.] Univ Coll Dublin, Dublin 4, Ireland.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Celik, Oe; Donato, D.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe; Donato, D.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France.
[Conrad, J.; Larsson, S.; Garde, M. Llena; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Larsson, S.; Garde, M. Llena; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy.
[Donato, D.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Donato, D.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Escande, L.; Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fukazawa, Y.; Itoh, R.; Katagiri, H.; Mizuno, T.; Nishino, S.; Uehara, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-30128 Toulouse 4, France.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Dermer, C. D.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[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.
[Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Schinzel, F. K.; Sokolovsky, K. V.; Kovalev, Y. Y.; Savolainen, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Sokolovsky, K. V.; Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117810, Russia.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.] 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.
[Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden.
[Berdyugin, A.; Kadenius, V.; Lindfors, E.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland.
[Boettcher, M.; Diltz, C.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Carraminana, A.; Carrasco, L.] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico.
[de la Fuente, E.] Univ Guadalajara, CUCEI, Inst Astron & Meteorol, Guadalajara 44130, Jalisco, Mexico.
[Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.] Aalto Univ Metsahovi Radio Observ, FIN-02540 Kylmala, Finland.
[Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
RP Ciprini, S (reprint author), Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
EM elisa.antolini@tiscali.it; stefano.ciprini@pg.infn.it;
davide.donato-1@nasa.gov; ksokolov@mpifr.de; gino.tosti@pg.infn.it
RI Johnson, Neil/G-3309-2014; Kovalev, Yuri/J-5671-2013; Funk,
Stefan/B-7629-2015; Sokolovsky, Kirill/D-2246-2015; Gargano,
Fabio/O-8934-2015; Loparco, Francesco/O-8847-2015; Johannesson,
Gudlaugur/O-8741-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016;
Orlando, E/R-5594-2016; Thompson, David/D-2939-2012; Gehrels,
Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012;
lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss,
Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer,
Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013;
Rando, Riccardo/M-7179-2013; Lahteenmaki, Anne/L-5987-2013; Hays,
Elizabeth/D-3257-2012;
OI Kovalev, Yuri/0000-0001-9303-3263; Funk, Stefan/0000-0002-2012-0080;
Sokolovsky, Kirill/0000-0001-5991-6863; Gargano,
Fabio/0000-0002-5055-6395; Loparco, Francesco/0000-0002-1173-5673;
Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko,
Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Frailis, Marco/0000-0002-7400-2135; Cutini,
Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X;
Gasparrini, Dario/0000-0002-5064-9495; Tramacere,
Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Thompson,
David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806;
Morselli, Aldo/0000-0002-7704-9553; giglietto,
nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214;
Savolainen, Tuomas/0000-0001-6214-1085; 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
FU ASI-INAF [I/047/8/0]; Associated Universities, Inc.; Academy of Finland
[212656, 210338]; NASA [NNX08AW56G, NNX09AU10G]
FX S.C. acknowledges funding by ASI-INAF grant No. I/047/8/0 related to
Fermi on-orbit activities.; This work includes observations obtained
with the NASA Swift gamma-ray burst Explorer. Swift is a MIDEX Gamma Ray
Burst mission led by NASA with participation of Italy and the UK. This
work includes observations obtained with NASA Rossi XTE satellite. The
ASM/RXTE teams at MIT and at the RXTE Science Operation Facility and
Guest Observer Facility at NASA's GSFC are gratefully thanked. This work
includes observations obtained with the Very Long Baseline Array, USA
(project code BK150). The National Radio Astronomy Observatory (NRAO
VLBA) is a facility of the National Science Foundation operated under
cooperative agreement by Associated Universities, Inc. This work
includes observations obtained with the 14 m Metsahovi Radio
Observatory, a separate research institute of the Helsinki University of
Technology. The Metsahovi team acknowledges the support from the Academy
of Finland to our observing projects (numbers 212656, 210338, and
others). This work includes observations obtained through the Tuorla
Blazar Monitoring Program, carried out with the KVA telescope on La
Palma, Canary Islands, and the 1 m telescope at Tuorla. Tuorla
Observatory is a division of the Department of Physics and Astronomy at
the University of Turku, Finland. This work includes observations
obtained through the optical monitoring of BL Lac and other blazars
using the 2.3 m Bok and 1.54 m Kuiper telescopes of Steward Observatory
that is supported by NASA/Fermi Guest Investigator grants NNX08AW56G and
NNX09AU10G. This work includes observations obtained with the 2.1 m
telescope of the OAGH (Observatorio Astrofisico Guillermo Haro), in the
state of Sonora, Mexico, operated by the Instituto Nacional de
Astrofisica, Optica y Electronica (INAOE), Mexico. This work includes
observations obtained with the 1.3 m McGraw-Hill Telescope of the
Michigan-Dartmouth-MIT (MDM) observatory, operated by University of
Michigan, Dartmouth College, Ohio State University, Ohio University,
Columbia University, in Arizona, USA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
PD APR 1
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SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900041
ER
PT J
AU Cook, AM
Whittet, DCB
Shenoy, SS
Gerakines, PA
White, DW
Chiar, JE
AF Cook, A. M.
Whittet, D. C. B.
Shenoy, S. S.
Gerakines, P. A.
White, D. W.
Chiar, J. E.
TI THE THERMAL EVOLUTION OF ICES IN THE ENVIRONMENTS OF NEWLY FORMED STARS:
THE CO2 DIAGNOSTIC
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; dust, extinction; evolution; infrared: ISM; ISM:
molecules; stars: pre-main sequence
ID SPITZER SPECTROSCOPIC SURVEY; YOUNG STELLAR OBJECTS; SOLID
CARBON-DIOXIDE; TAURUS DARK CLOUDS; INFRARED-SPECTROSCOPY; MOLECULAR
CLOUD; GRAIN MANTLES; INTERSTELLAR EXTINCTION; BACKGROUND STARS;
SPACE-TELESCOPE
AB Archival data from the Infrared Spectrometer of the Spitzer Space Telescope are used to study the 15 mu m absorption feature of solid CO2 toward 28 young stellar objects (YSOs) of approximately solar mass. Fits to the absorption profile using laboratory spectra enable categorization according to the degree of thermal processing of the ice matrix that contains the CO2. The majority of YSOs in our sample (20 out of 28) are found to be consistent with a combination of polar (H2O-rich) and nonpolar (CO-rich) ices at low temperature; the remainder exhibit profile structure consistent with partial crystallization as the result of significant heating. Ice-phase column densities of CO2 are determined and compared with those of other species. Lines of sight with crystallization signatures in their spectra are found to be systematically deficient in solid-phase CO, as expected if CO is being sublimated in regions where the ices are heated to crystallization temperatures. Significant variation is found in the CO2 abundance with respect to both H2O (the dominant ice constituent) and total dust column (quantified by the extinction, AV). YSOs in our sample display typically higher CO2 concentrations (independent of evidence for thermal processing) in comparison to quiescent regions of the prototypical cold molecular cloud. This suggests that enhanced CO2 production is driven by photochemical reactions in proximity to some YSOs, and that photoprocessing and thermal processing may occur independently.
C1 [Cook, A. M.; Whittet, D. C. B.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Troy, NY 12180 USA.
[Cook, A. M.; Whittet, D. C. B.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA.
[Shenoy, S. S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Gerakines, P. A.; White, D. W.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA.
[Chiar, J. E.] SETI Inst, Mountain View, CA 94043 USA.
RP Cook, AM (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA.
RI Gerakines, Perry/D-2226-2012; Gerakines, Perry/B-9705-2009;
OI Gerakines, Perry/0000-0002-9667-5904; Whittet,
Douglas/0000-0001-8539-3891
FU Spitzer [1264149, 1290823]; NASA [NNX07AK38G]; NASA Astrobiology
Institute [NNA09DA80A]; NASA New York
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA.
Financial support for this research was provided by the Spitzer General
Observer and Archival Research Programs (JPL/Caltech Support Agreements
nos. 1264149 and 1290823), the NASA Exobiology and Evolutionary Biology
program (grant NNX07AK38G), the NASA Astrobiology Institute (grant
NNA09DA80A), and the NASA New York Space Grant Consortium. We are
grateful to an anonymous referee for helpful comments.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
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SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900064
ER
PT J
AU Efremova, BV
Bianchi, L
Thilker, DA
Neill, JD
Burgarella, D
Wyder, TK
Madore, BF
Rey, SC
Barlow, TA
Conrow, T
Forster, K
Friedman, PG
Martin, DC
Morrissey, P
Neff, SG
Schiminovich, D
Seibert, M
Small, T
AF Efremova, Boryana V.
Bianchi, Luciana
Thilker, David A.
Neill, James D.
Burgarella, Denis
Wyder, Ted K.
Madore, Barry F.
Rey, Soo-Chang
Barlow, Tom A.
Conrow, Tim
Forster, Karl
Friedman, Peter G.
Martin, D. Christopher
Morrissey, Patrick
Neff, Susan G.
Schiminovich, David
Seibert, Mark
Small, Todd
TI THE RECENT STAR FORMATION IN NGC 6822: AN ULTRAVIOLET STUDY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 6822); galaxies: stellar content; Local Group;
stars: formation; ultraviolet: stars
ID HUBBLE-SPACE-TELESCOPE; H-II REGIONS; CURRENTLY FORMING STARS; INITIAL
MASS FUNCTION; EMISSION-LINE STARS; GALAXY NGC-6822; MAGELLANIC-CLOUD;
DUST ATTENUATION; DWARF GALAXIES; LMC CLUSTERS
AB We characterize the star formation in the low-metallicity galaxy NGC 6822 over the past few hundred million years, using GALEX far-UV (FUV, 1344-1786 angstrom) and near-UV (NUV, 1771-2831 angstrom) imaging, and ground-based H alpha imaging. From the GALEX FUV image, we define 77 star-forming (SF) regions with area > 860 pc(2), and surface brightness less than or similar to 26.8 mag (AB) arcsec(-2), within 0 degrees.2 (1.7 kpc) of the center of the galaxy. We estimate the extinction by interstellar dust in each SF region from resolved photometry of the hot stars it contains: E(B - V) ranges from the minimum foreground value of 0.22 mag up to 0.66 +/- 0.21 mag. The integrated FUV and NUV photometry, compared with stellar population models, yields ages of the SF complexes up to a few hundred Myr, and masses from 2 x 10(2) M-circle dot to 1.5 x 10(6) M-circle dot. The derived ages and masses strongly depend on the assumed type of interstellar selective extinction, which we find to vary across the galaxy. The total mass of the FUV-defined SF regions translates into an average star formation rate (SFR) of 1.4 x 10(-2) M-circle dot yr(-1) over the past 100 Myr, and SFR = 1.0 x 10(-2) M-circle dot yr(-1) in the most recent 10 Myr. The latter is in agreement with the value that we derive from the H alpha luminosity, SFR = 0.008 M-circle dot yr(-1). The SFR in the most recent epoch becomes higher if we add the SFR = 0.02 M-circle dot yr(-1) inferred from far-IR measurements, which trace star formation still embedded in dust (age less than or similar to a few Myr).
C1 [Efremova, Boryana V.; Bianchi, Luciana; Thilker, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Neill, James D.; Wyder, Ted K.; Barlow, Tom A.; Conrow, Tim; Forster, Karl; Friedman, Peter G.; Martin, D. Christopher; Morrissey, Patrick; Small, Todd] CALTECH, Pasadena, CA 91125 USA.
[Burgarella, Denis] Lab Astrophys Marseille, F-13376 Marseille 12, France.
[Madore, Barry F.; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Rey, Soo-Chang] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea.
[Rey, Soo-Chang; Neff, Susan G.] NASA, Goddard Space Flight Ctr, Lab Astron & Solar Phys, Greenbelt, MD 20771 USA.
[Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA.
RP Efremova, BV (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM boryana@pha.jhu.edu; bianchi@pha.jhu.edu
FU NASA [NAS5-26555]; NASA Office of Space Science [NAG5-7584]; NRF of
Korea
FX The GALEX 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. GALEX (The Galaxy Evolution
Explorer) is a NASA Small Explorer, launched in 2003 April. We
gratefully acknowledge NASA's support for construction, operation, and
science analysis of the GALEX mission, developed in cooperation with the
Centre National d'Etudes Spatiales of France and the Korean Ministry of
Science and Technology. The H alpha image used in this paper was
obtained by Massey et al. (2007a) as part of the Survey of Local Group
Galaxies Currently Forming Stars and downloaded from
http://www.archive.noao.edu/nsa/. S.-C.R. is supported by the NRF of
Korea to the Center for Galaxy Evolution Research.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900028
ER
PT J
AU Gruesbeck, JR
Lepri, ST
Zurbuchen, TH
Antiochos, SK
AF Gruesbeck, Jacob R.
Lepri, Susan T.
Zurbuchen, Thomas H.
Antiochos, Spiro K.
TI CONSTRAINTS ON CORONAL MASS EJECTION EVOLUTION FROM IN SITU OBSERVATIONS
OF IONIC CHARGE STATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atomic processes; plasmas; solar wind; Sun: coronal mass ejections
(CMEs)
ID ADVANCED COMPOSITION EXPLORER; SOLAR-WIND; PARTICLE-ACCELERATION;
MAGNETIC-FIELD; FLARE; TEMPERATURE; SIGNATURES; PLASMA; MODEL; LASCO
AB We present a novel procedure for deriving the physical properties of coronal mass ejections (CMEs) in the corona. Our methodology uses in situ measurements of ionic charge states of C, O, Si, and Fe in the heliosphere and interprets them in the context of a model for the early evolution of interplanetary CME (ICME) plasma, between 2 and 5R(circle dot). We find that the data are best fit by an evolution that consists of an initial heating of the plasma, followed by an expansion that ultimately results in cooling. The heating profile is consistent with a compression of coronal plasma due to flare reconnection jets and an expansion cooling due to the ejection, as expected from the standard CME/flare model. The observed frozen-in ionic charge states reflect this time history and, therefore, provide important constraints for the heating and expansion timescales, as well as the maximum temperature the CME plasma is heated to during its eruption. Furthermore, our analysis places severe limits on the possible density of CME plasma in the corona. We discuss the implications of our results for CME models and for future analysis of ICME plasma composition.
C1 [Gruesbeck, Jacob R.; Lepri, Susan T.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gruesbeck, JR (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM jagruesb@umich.edu
RI Antiochos, Spiro/D-4668-2012; Lepri, Susan/I-8611-2012
OI Antiochos, Spiro/0000-0003-0176-4312;
FU NASA [NNX08AI11G, NNX07AB99G, NNX08AM64G]; GSRP
FX This work used the SOHO/LASCO CME catalog developed by NASA, NRL, and
the Catholic University of America. SOHO is a project of international
cooperation between ESA and NASA. This work was performed, in part, with
support from NASA grants NNX08AI11G, NNX07AB99G, and NNX08AM64G, as well
as the GSRP program. T.H.Z. acknowledges the hospitality of the
International Space Science Institute, where much of this work was
performed. S.K.A. was supported, in part by the NASA HTP and TR&T
Programs. The authors thank Eric Christian for helpful discussions and
comments on the manuscript. The authors thank Katherine Baldwin and Jim
Raines for their early work, which was a foundation for this study.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2011
VL 730
IS 2
AR 103
DI 10.1088/0004-637X/730/2/103
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900043
ER
PT J
AU Kasliwal, MM
Kulkarni, SR
Arcavi, I
Quimby, RM
Ofek, EO
Nugent, P
Jacobsen, J
Gal-Yam, A
Green, Y
Yaron, O
Fox, DB
Howell, JL
Cenko, SB
Kleiser, I
Bloom, JS
Miller, A
Li, WD
Filippenko, AV
Starr, D
Poznanski, D
Law, NM
Helou, G
Frail, DA
Neill, JD
Forster, K
Martin, DC
Tendulkar, SP
Gehrels, N
Kennea, J
Sullivan, M
Bildsten, L
Dekany, R
Rahmer, G
Hale, D
Smith, R
Zolkower, J
Velur, V
Walters, R
Henning, J
Bui, K
McKenna, D
Blake, C
AF Kasliwal, Mansi M.
Kulkarni, Shri R.
Arcavi, Iair
Quimby, Robert M.
Ofek, Eran O.
Nugent, Peter
Jacobsen, Janet
Gal-Yam, Avishay
Green, Yoav
Yaron, Ofer
Fox, Derek B.
Howell, Jacob L.
Cenko, S. Bradley
Kleiser, Io
Bloom, Joshua S.
Miller, Adam
Li, Weidong
Filippenko, Alexei V.
Starr, Dan
Poznanski, Dovi
Law, Nicholas M.
Helou, George
Frail, Dale A.
Neill, James D.
Forster, Karl
Martin, D. Christopher
Tendulkar, Shriharsh P.
Gehrels, Neil
Kennea, Jamie
Sullivan, Mark
Bildsten, Lars
Dekany, Richard
Rahmer, Gustavo
Hale, David
Smith, Roger
Zolkower, Jeff
Velur, Viswa
Walters, Richard
Henning, John
Bui, Kahnh
McKenna, Dan
Blake, Cullen
TI PTF 10fqs: A LUMINOUS RED NOVA IN THE SPIRAL GALAXY MESSIER 99
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: AGB and post-AGB; stars: mass-loss; supernovae: general;
supernovae: individual (PTF 10fqs); surveys
ID OBSERVATORY SUPERNOVA SEARCH; SN 2008S; OPTICAL TRANSIENT; NEARBY
GALAXIES; NGC 300; TELESCOPE; EVOLUTION; EMISSION; SPITZER; PERFORMANCE
AB The Palomar Transient Factory (PTF) is systematically charting the optical transient and variable sky. A primary science driver of PTF is building a complete inventory of transients in the local universe (distance less than 200 Mpc). Here, we report the discovery of PTF 10fqs, a transient in the luminosity "gap" between novae and supernovae. Located on a spiral arm of Messier 99, PTF 10fqs has a peak luminosity of M-r = -12.3, red color (g - r = 1.0), and is slowly evolving (decayed by 1 mag in 68 days). It has a spectrum dominated by intermediate-width Ha (approximate to 930 km s(-1)) and narrow calcium emission lines. The explosion signature (the light curve and spectra) is overall similar to that of M85 OT2006-1, SN 2008S, and NGC 300 OT. The origin of these events is shrouded in mystery and controversy (and in some cases, in dust). PTF 10fqs shows some evidence of a broad feature (around 8600 angstrom) that may suggest very large velocities (approximate to 10,000 km s(-1)) in this explosion. Ongoing surveys can be expected to find a few such events per year. Sensitive spectroscopy, infrared monitoring, and statistics (e.g., disk versus bulge) will eventually make it possible for astronomers to unravel the nature of these mysterious explosions.
C1 [Kasliwal, Mansi M.; Kulkarni, Shri R.; Quimby, Robert M.; Ofek, Eran O.; Neill, James D.; Forster, Karl; Martin, D. Christopher; Tendulkar, Shriharsh P.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Arcavi, Iair; Gal-Yam, Avishay; Green, Yoav; Yaron, Ofer] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, IL-76100 Rehovot, Israel.
[Nugent, Peter; Jacobsen, Janet; Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Fox, Derek B.; Howell, Jacob L.] Penn State Univ, Eberly Coll Sci, University Pk, PA 16802 USA.
[Cenko, S. Bradley; Kleiser, Io; Bloom, Joshua S.; Miller, Adam; Li, Weidong; Filippenko, Alexei V.; Starr, Dan; Poznanski, Dovi] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Law, Nicholas M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Helou, George] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Frail, Dale A.] Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kennea, Jamie] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Sullivan, Mark] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Bildsten, Lars] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Bildsten, Lars] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Dekany, Richard; Rahmer, Gustavo; Hale, David; Smith, Roger; Zolkower, Jeff; Velur, Viswa; Walters, Richard; Henning, John; Bui, Kahnh; McKenna, Dan] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA.
[Blake, Cullen] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Kasliwal, MM (reprint author), CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
RI Gehrels, Neil/D-2971-2012; Green, Yoav/L-5874-2015;
OI Green, Yoav/0000-0002-0809-6575; Sullivan, Mark/0000-0001-9053-4820
FU Gordon and Betty Moore Foundation; Israel Science Foundation; US-Israel
Binational Science Foundation; Weizmann-UK; Marie Curie IRG fellowship;
Peter and Patricia Gruber Award; Benoziyo Center for Astrophysics;
Yeda-Sela center at the Weizmann Institute; National Science Foundation
(NSF) [AST-0908886, PHY 05-51164, AST07-07633]; Sylvia & Jim Katzman
Foundation; Richard & Rhoda Goldman Fund; Gary and Cynthia Bengier;
TABASGO Foundation; NASA through Spitzer [1322321]; Space Telescope
Science Institute [AR-11248]; NASA [NAS 5-26555]; DOE; Einstein
fellowship; Harvard University; University of Virginia; Associated
Universities, Inc.
FX M.M.K. thanks the Gordon and Betty Moore Foundation for a Hale
Fellowship in support of graduate study. The Weizmann Institute PTF
participation is supported in part by the Israel Science Foundation via
grants to A.G.Y. The Weizmann-Caltech collaborative PTF effort is
supported by the US-Israel Binational Science Foundation. A.G.Y. and M.
S. are jointly supported by the "making connections" Weizmann-UK
program. A.G.Y. further acknowledges support by a Marie Curie IRG
fellowship and the Peter and Patricia Gruber Award, as well as funding
by the Benoziyo Center for Astrophysics and the Yeda-Sela center at the
Weizmann Institute. A.V.F.'s group and KAIT are supported by National
Science Foundation (NSF) grant AST-0908886, the Sylvia & Jim Katzman
Foundation, the Richard & Rhoda Goldman Fund, Gary and Cynthia Bengier,
and the TABASGO Foundation; additional funding was provided by NASA
through Spitzer grant 1322321, as well as HST grant AR-11248 from the
Space Telescope Science Institute, which is operated by Associated
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555. J.S.B. and his group are partially funded by a DOE SciDAC
grant. E.O.O. and D. P. are supported by the Einstein fellowship. L. B.
is supported by the National Science Foundation under grants PHY
05-51164 and AST07-07633.; The Hobby-Eberly Telescope (HET) is a joint
project of the University of Texas at Austin, the Pennsylvania State
University, Stanford University, Ludwig-Maximillians-Universitat
Munchen, and Georg-August-Universitat Gottingen. The HET is named in
honor of its principal benefactors, William P. Hobby and Robert E.
Eberly. The Marcario LRS is named for Mike Marcario of High Lonesome
Optics, who fabricated several optics for the instrument but died before
its completion; it is a joint project of the Hobby-Eberly Telescope
partnership and the Instituto de Astronomia de la Universidad Nacional
Autonoma de Mexico. GALEX (Galaxy Evolution Explorer) is a NASA Small
Explorer, launched in 2003 April. We gratefully acknowledge NASA's
support for construction, operation, and science analysis for the GALEX
mission, developed in cooperation with the Centre National d'Etudes
Spatiales of France and the Korean Ministry of Science and Technology.
PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO)
and was made possible by a grant from the Harvard University Milton
Fund, the camera loan from the University of Virginia, and the continued
support of the SAO and UC Berkeley. The Expanded Very Large Array is
operated by the National Radio Astronomy Observatory, a facility of the
NSF operated under cooperative agreement by Associated Universities,
Inc.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2011
VL 730
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AR 134
DI 10.1088/0004-637X/730/2/134
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900074
ER
PT J
AU Livingstone, MA
Ng, CY
Kaspi, VM
Gavriil, FP
Gotthelf, EV
AF Livingstone, Margaret A.
Ng, C. -Y.
Kaspi, Victoria M.
Gavriil, Fotis P.
Gotthelf, E. V.
TI POST-OUTBURST OBSERVATIONS OF THE MAGNETICALLY ACTIVE PULSAR J1846-0258.
A NEW BRAKING INDEX, INCREASED TIMING NOISE, AND RADIATIVE RECOVERY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; pulsars: individual (PSR J1846-0258); supernovae:
individual (Kes 75); X-rays: stars
ID PROPORTIONAL COUNTER ARRAY; ROTATION-POWERED PULSAR; REMNANT KESTEVEN
75; X-RAY PULSARS; SPIN-DOWN; PSR J1846-0258; MAGNETAR SGR-1806-20;
NEUTRON-STARS; VELA PULSAR; WIND NEBULA
AB The similar to 800 year old pulsar J1846-0258 is a unique transition object between rotation-powered pulsars and magnetars: though behaving like a rotation-powered pulsar most of the time, in 2006 it exhibited a distinctly magnetar-like outburst accompanied by a large glitch. Here, we present X-ray timing observations taken with the Rossi X-ray Timing Explorer over a 2.2 year period after the X-ray outburst and glitch had recovered. We observe that the braking index of the pulsar, previously measured to be n = 2.65 +/- 0.01, is now n = 2.16 +/- 0.13, a decrease of 18% +/- 5%. We also note a persistent increase in the timing noise relative to the pre-outburst level. Despite the timing changes, a 2009 Chandra X-ray Observatory observation shows that the X-ray flux and spectrum of the pulsar and its wind nebula are consistent with the quiescent levels observed in 2000.
C1 [Livingstone, Margaret A.; Ng, C. -Y.; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Gavriil, Fotis P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Gavriil, Fotis P.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
[Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
RP Livingstone, MA (reprint author), McGill Univ, Dept Phys, Rutherford Phys Bldg, Montreal, PQ H3A 2T8, Canada.
EM maggie@physics.mcgill.ca
RI Ng, Chi Yung/A-7639-2013
OI Ng, Chi Yung/0000-0002-5847-2612
FU NSERC [228738-03]; FQRNT; CIFAR
FX We thank A. Beloborodov, A. Melatos, and an anonymous referee for
comments that improved the manuscript. This research made use of data
obtained from the High Energy Astrophysics Science Archive Research
Center Online Service, provided by the NASA-Goddard Space Flight Center.
C.Y.N. is a CRAQ postdoctoral fellow. V.M.K. holds the Lorne Trottier
Chair in Astrophysics and Cosmology and a Canada Research Chair in
Observational Astrophysics. Funding for this work was provided by NSERC
Discovery Grant Rgpin 228738-03, FQRNT, and CIFAR.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2011
VL 730
IS 2
AR 66
DI 10.1088/0004-637X/730/2/66
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900006
ER
PT J
AU Roy, A
Ade, PAR
Bock, JJ
Brunt, CM
Chapin, EL
Devlin, MJ
Dicker, SR
France, K
Gibb, AG
Griffin, M
Gundersen, JO
Halpern, M
Hargrave, PC
Hughes, DH
Klein, J
Marsden, G
Martin, PG
Mauskopf, P
Netterfield, CB
Olmi, L
Patanchon, G
Rex, M
Scott, D
Semisch, C
Truch, MDP
Tucker, C
Tucker, GS
Viero, MP
Wiebe, DV
AF Roy, Arabindo
Ade, Peter A. R.
Bock, James J.
Brunt, Christopher M.
Chapin, Edward L.
Devlin, Mark J.
Dicker, Simon R.
France, Kevin
Gibb, Andrew G.
Griffin, Matthew
Gundersen, Joshua O.
Halpern, Mark
Hargrave, Peter C.
Hughes, David H.
Klein, Jeff
Marsden, Gaelen
Martin, Peter G.
Mauskopf, Philip
Netterfield, Calvin B.
Olmi, Luca
Patanchon, Guillaume
Rex, Marie
Scott, Douglas
Semisch, Christopher
Truch, Matthew D. P.
Tucker, Carole
Tucker, Gregory S.
Viero, Marco P.
Wiebe, Donald V.
TI DECONVOLUTION OF IMAGES FROM BLAST 2005: INSIGHT INTO THE K3-50 AND IC
5146 STAR-FORMING REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation; submillimeter: general; techniques: image processing
ID DARK CLOUD COMPLEX; APERTURE-SUBMILLIMETER-TELESCOPE; GALACTIC PLANE
SURVEY; BLIND DECONVOLUTION; SUPERNOVA REMNANT; MOLECULAR CLOUDS;
MAXIMUM-ENTROPY; LUCY ALGORITHM; CO OUTFLOWS; RESTORATION
AB We present an implementation of the iterative flux-conserving Lucy-Richardson (L-R) deconvolution method of image restoration for maps produced by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST). Compared to the direct Fourier transform method of deconvolution, the L-R operation restores images with better-controlled background noise and increases source detectability. Intermediate iterated images are useful for studying extended diffuse structures, while the later iterations truly enhance point sources to near the designed diffraction limit of the telescope. The L-R method of deconvolution is efficient in resolving compact sources in crowded regions while simultaneously conserving their respective flux densities. We have analyzed its performance and convergence extensively through simulations and cross-correlations of the deconvolved images with available high-resolution maps. We present new science results from two BLAST surveys, in the Galactic regions K3-50 and IC 5146, further demonstrating the benefits of performing this deconvolution. We have resolved three clumps within a radius of 4.'5 inside the star-forming molecular cloud containing K3-50. Combining the well-resolved dust emission map with available multi-wavelength data, we have constrained the spectral energy distributions (SEDs) of five clumps to obtain masses (M), bolometric luminosities (L), and dust temperatures (T). The L-M diagram has been used as a diagnostic tool to estimate the evolutionary stages of the clumps. There are close relationships between dust continuum emission and both 21 cm radio continuum and (CO)-C-12 molecular line emission. The restored extended large-scale structures in the Northern Streamer of IC 5146 have a strong spatial correlation with both SCUBA and high-resolution extinction images. A dust temperature of 12 K has been obtained for the central filament. We report physical properties of ten compact sources, including six associated protostars, by fitting SEDs to multi-wavelength data. All of these compact sources are still quite cold (typical temperature below similar to 16 K) and are above the critical Bonner-Ebert mass. They have associated low-power young stellar objects. Further evidence for starless clumps has also been found in the IC 5146 region.
C1 [Roy, Arabindo; Netterfield, Calvin B.; Viero, Marco P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Tucker, Carole] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, James J.; Viero, Marco P.] CALTECH, Pasadena, CA 91125 USA.
[Brunt, Christopher M.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Chapin, Edward L.; Gibb, Andrew G.; Halpern, Mark; Marsden, Gaelen; Scott, Douglas; Wiebe, Donald V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Rex, Marie; Semisch, Christopher; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Gundersen, Joshua O.] Univ Miami, Dept Phys, Carol Gables, FL 33146 USA.
[Hughes, David H.] INAOE, Puebla, Mexico.
[Martin, Peter G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Olmi, Luca] Univ Puerto Rico, Dept Phys, UPR Stn, San Juan, PR 00936 USA.
[Olmi, Luca] Ist Radioastron, I-50125 Florence, Italy.
[Patanchon, Guillaume] Lab APC, F-75205 Paris, France.
[Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
RP Roy, A (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
EM aroy@cita.utoronto.ca
RI Klein, Jeffrey/E-3295-2013;
OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840
FU NASA [NAG5-12785, NAG5-13301, NNGO-6GI11G]; Canadian Space Agency (CSA);
UK Particle Physics & Astronomy Research Council (PPARC); Canada's
Natural Sciences and Engineering Research Council (NSERC)
FX The BLAST collaboration acknowledges the support of NASA through grant
numbers NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space
Agency (CSA), the UK Particle Physics & Astronomy Research Council
(PPARC), and Canada's Natural Sciences and Engineering Research Council
(NSERC). We also thank the Columbia Scientific Balloon Facility (CSBF)
staff for their outstanding work.
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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 APR 1
PY 2011
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AR 142
DI 10.1088/0004-637X/730/2/142
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900082
ER
PT J
AU Savage, SL
McKenzie, DE
AF Savage, Sabrina L.
McKenzie, David E.
TI QUANTITATIVE EXAMINATION OF A LARGE SAMPLE OF SUPRA-ARCADE DOWNFLOWS IN
ERUPTIVE SOLAR FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun:
magnetic topology; Sun: UV radiation; Sun: X-rays, gamma rays
ID CORONAL MASS EJECTION; FIELD LINE SHRINKAGE; CURRENT SHEET;
MAGNETIC-FIELDS; RECONNECTION; EMISSIONS; MOTIONS; HINODE; MODEL
AB Sunward-flowing voids above post-coronal mass ejection flare arcades were first discovered using the soft X-ray telescope aboard Yohkoh and have since been observed with TRACE (extreme ultraviolet (EUV)), SOHO/LASCO (white light), SOHO/SUMER (EUV spectra), and Hinode/XRT (soft X-rays). Supra-arcade downflow (SAD) observations suggest that they are the cross-sections of thin flux tubes retracting from a reconnection site high in the corona. Supra-arcade downflowing loops (SADLs) have also been observed under similar circumstances and are theorized to be SADs viewed from a perpendicular angle. Although previous studies have focused on dark flows because they are easier to detect and complementary spectral data analysis reveals their magnetic nature, the signal intensity of the flows actually ranges from dark to bright. This implies that newly reconnected coronal loops can contain a range of hot plasma density. Previous studies have presented detailed SAD observations for a small number of flares. In this paper, we present a substantial SADs and SADLs flare catalog. We have applied semiautomatic detection software to several of these events to detect and track individual downflows thereby providing statistically significant samples of parameters such as velocity, acceleration, area, magnetic flux, shrinkage energy, and reconnection rate. We discuss these measurements (particularly the unexpected result of the speeds being an order of magnitude slower than the assumed Alfven speed), how they were obtained, and potential impact on reconnection models.
C1 [Savage, Sabrina L.] Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Savage, Sabrina L.; McKenzie, David E.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RP Savage, SL (reprint author), Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 671, Greenbelt, MD 20771 USA.
FU NASA [NNM07AB07C]; Harvard-Smithsonian Astrophysical Observatory
FX This work was supported by NASA under contract NNM07AB07C with the
Harvard-Smithsonian Astrophysical Observatory. The authors thank Drs. D.
Longcope, C. Kankelborg, J. Qiu, A. Des Jardins, and the anonymous
referee for constructive conversations and comments. 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).
Yohkoh data are provided courtesy of the NASA-supported Yohkoh Legacy
Archive at Montana State University.
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PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2011
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AR 98
DI 10.1088/0004-637X/730/2/98
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900038
ER
PT J
AU Singal, J
Fixsen, DJ
Kogut, A
Levin, S
Limon, M
Lubin, P
Mirel, P
Seiffert, M
Villela, T
Wollack, E
Wuensche, CA
AF Singal, J.
Fixsen, D. J.
Kogut, A.
Levin, S.
Limon, M.
Lubin, P.
Mirel, P.
Seiffert, M.
Villela, T.
Wollack, E.
Wuensche, C. A.
TI THE ARCADE 2 INSTRUMENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; instrumentation: detectors; radio
continuum: galaxies
ID TEMPERATURE; GHZ; CALIBRATOR; RADIATION; DESIGN; COBE
AB The second generation Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE 2) instrument is a balloon-borne experiment to measure the radiometric temperature of the cosmic microwave background and Galactic and extragalactic emission at six frequencies from 3 to 90 GHz. ARCADE 2 utilizes a double-nulled design where emission from the sky is compared to that from an external cryogenic full-aperture blackbody calibrator by cryogenic switching radiometers containing internal blackbody reference loads. In order to further minimize sources of systematic error, ARCADE 2 features a cold fully open aperture with all radiometrically active components maintained at near 2.7 K without windows or other warm objects, achieved through a novel thermal design. We discuss the design and performance of the ARCADE 2 instrument in its 2005 and 2006 flights.
C1 [Singal, J.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Singal, J.] Stanford Univ, Menlo Pk, CA 94025 USA.
[Fixsen, D. J.] Univ Maryland, Dept Phys, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Levin, S.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Limon, M.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Lubin, P.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Villela, T.; Wuensche, C. A.] Inst Nacl Pesquisas Espaciais, Div Astrophys, BR-12245970 Sao Jose Dos Campos, SP, Brazil.
RP Singal, J (reprint author), SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
EM jsingal@stanford.edu
RI Tecnologias espaciai, Inct/I-2415-2013; Wollack, Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698
FU NASA's Science Mission Directorate; National Aeronautics and Space
Administration; CNPq [466184/00-0, 305219-2004-9, 303637/2007-2-FA,
307433/2004-8-FA]
FX We thank the staff at CSBF for launch support. We thank Victor Kulesh
for contributions to the ground software, and Adam Bushmaker, Jane
Cornett, Paul Cursey, Sarah Fixsen, Luke Lowe, and Alexandre Rischard
for their work on the project. We thank the Cryogenics Branch at GSFC
for supporting the ARCADE 2 design and thermometer calibration, Todd
Gaier for the 90 GHz amplifiers, and Custom Microwave, Bechdon, Inc.,
Flight Fab, and JMD for fabrication of components. This research has
been supported by NASA's Science Mission Directorate under the Astronomy
and Physics Research and Analysis suborbital program. The research
described in this paper was performed in part at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. T. V. acknowledges
support from CNPq grants 466184/00-0, 305219-2004-9, and
303637/2007-2-FA, and the technical support from Luiz Reitano. C.A.W.
acknowledges support from CNPq grant 307433/2004-8-FA.
NR 15
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2011
VL 730
IS 2
AR 138
DI 10.1088/0004-637X/730/2/138
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735TR
UT WOS:000288441900078
ER
PT J
AU Jeon, HS
Cho, S
Kwak, YS
Chung, JK
Park, JU
Lee, DK
Kuzmicz-Cieslak, M
AF Jeon, H. S.
Cho, S.
Kwak, Y. S.
Chung, J. K.
Park, J. U.
Lee, D. K.
Kuzmicz-Cieslak, M.
TI Mass density of the upper atmosphere derived from Starlette's Precise
Orbit Determination with Satellite Laser Ranging
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article
DE Mass density; Starlette; Precise Orbit Determination; Satellite Laser
Ranging; MSIS models; Geomagnetic activity
ID ACCELEROMETER DATA; MAGNETIC STORMS; NEUTRAL DENSITY; SOLAR; CHAMP;
MODEL
AB The atmospheric mass density of the upper atmosphere from the spherical Starlette satellite's Precise Orbit Determination is first derived with Satellite Laser Ranging measurements at 815 to 1115 km during strong solar and geomagnetic activities. Starlette's orbit is determined using the improved orbit determination techniques combining optimum parameters with a precise empirical drag application to a gravity field. MSIS-86 and NRLMSISE-00 atmospheric density models are compared with the Starlette drag-derived atmospheric density of the upper atmosphere. It is found that the variation in the Starlette's drag coefficient above 800 km corresponds well with the level of geomagnetic activity. This represents that the satellite orbit is mainly perturbed by the Joule heating from geomagnetic activity at the upper atmosphere. This result concludes that MSIS empirical models strongly underestimate the mass density of the upper atmosphere as compared to the Starlette drag-derived atmospheric density during the geomagnetic storms. We suggest that the atmospheric density models should be analyzed with higher altitude acceleration data for a better understanding of long-term solar and geomagnetic effects.
C1 [Jeon, H. S.] Univ Sci & Technol, Taejon 305333, South Korea.
[Jeon, H. S.; Cho, S.; Kwak, Y. S.; Chung, J. K.; Park, J. U.] Korea Astron & Space Sci Inst, Div Space Sci, Taejon 305348, South Korea.
[Jeon, H. S.; Lee, D. K.] Korean Air Force Headquarters, Gyeryong 321919, Chungnam, South Korea.
[Kuzmicz-Cieslak, M.] UMBC & NASA Goddard 698, NASA, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA.
RP Jeon, HS (reprint author), Univ Sci & Technol, Taejon 305333, South Korea.
EM ewmann@kasi.re.kr
FU NASA Goddard Earth Science and Technology Center (GEST); Goddard Space
Flight Center, Greenbelt
FX This work was supported by the NASA Goddard Earth Science and Technology
Center (GEST) from the Goddard Space Flight Center, Greenbelt. The
authors thank the International Laser Ranging Service (ILRS) stations
and data centers for the high quality global SLR observations. The
author appreciates Dr. K.A. Firoz, Mr. J.H. Baek, and Ms. W.K. Lee in
KASI for generous assistances. We are grateful to honorable reviewers
for their valuable comments and suggestions that indeed developed the
quality of this study.
NR 30
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U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD APR
PY 2011
VL 332
IS 2
BP 341
EP 351
DI 10.1007/s10509-010-0528-2
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732UP
UT WOS:000288215500014
ER
PT J
AU Sakowski, C
Starc, V
Smith, SM
Schlegel, TT
AF Sakowski, Chris
Starc, Vito
Smith, Scott M.
Schlegel, Todd T.
TI Sedentary Long-Duration Head-Down Bed Rest and ECG Repolarization
Heterogeneity
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE electrocardiogram; QRS-T angle; QT variability; T-wave complexity;
spatial ventricular gradient
ID QRS-T ANGLE; LEFT-VENTRICULAR HYPERTROPHY; CORONARY-ARTERY-DISEASE;
QT-INTERVAL VARIABILITY; PREDICTS CARDIAC DEATH; TORSADES-DE-POINTES;
NUTRITIONAL-STATUS; WAVE ALTERNANS; SPACE-FLIGHT; ELECTROCARDIOGRAPHY
AB SAKOWSKI C, STARC V, SMITH SM, SCHLEGEL TT. Sedentary long-duration head-down bed rest and ECG repolarization heterogeneity. Aviat Space Environ Med 2011; 82:416-23.
Background: We studied the effects of 90 d of 6 degrees head-down bed rest (HDBR) on cardiac autonomic and advanced electrocardiographic (ECG) function, especially on repolarization heterogeneity as assessed by beat-to-beat QT interval variability (QTV), T-wave complexity, and 3-dimensional ECG. Based on prior observations of lengthening of the QTc interval during long-duration spaceflight, we hypothesized that abnormalities in ECG repolarization would also occur during long-duration HDBR. Methods: During controlled breathing, 5-min supine high-fidelity 12-lead ECGs were obtained from 20 healthy subjects (14 men and 6 women) together with measurements of plasma volume and electrolytes at 5 points in time: within 10 d before; 28-30, 60, and 90 d into; and 3-5 d after HDBR. Results: By repeated measures ANOVA, 90 d of sedentary HDBR significantly increased the QTV index (from 1.87 +/- 0.33 to - 1.53 +/- 0.39 units), the index of unexplained QTV (from 0.61 +/- 0.48 to 1.21 +/- 0.40 units), the T-wave complexity intradipolar ratio (from 0.344 +/- 0.260 to 2.04 +/- 4.01%), and the spatial QRS-T angle (from 49.1 +/- 23.8 to 58.7 +/- 31.0 degrees), and significantly decreased the spatial ventricular gradient (from 91.3 +/- 26.5 to 59.1 +/- 23.0 mV . ms(-1)). These changes resolved in part by 3-5 d after resumption of ambulation, but unlike concomitant changes in the QTc interval itself and in heart rate variability, they did not significantly relate to changes in electrolytes or plasma volume. Conclusions: Sedentary, long-duration HDBR reversibly increases ECG repolarization heterogeneity and by inference ventricular arrhythmic risk.
C1 [Smith, Scott M.; Schlegel, Todd T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Sakowski, Chris] Univ Texas Med Branch, Galveston, TX USA.
[Starc, Vito] Univ Ljubljana, Fac Med, Inst Physiol, Ljubljana, Slovenia.
RP Schlegel, TT (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK272, Houston, TX 77058 USA.
EM todd.t.schlegel@nasa.gov
FU UTMB; USA-Slovenia Cooperation in Science and Technology; Johnson Space
Center; Human Test Subject Facility
FX This research was supported by the UTMB Medical Student Summer Research
Program (CS); the USA-Slovenia Cooperation in Science and Technology
(VS, TTS); and the Johnson Space Center Flight Analogs Project (DSM,
SMS, TTS) and Human Test Subject Facility (TTS).
NR 45
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U2 3
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD APR
PY 2011
VL 82
IS 4
BP 416
EP 423
DI 10.3357/ASEM.2945.2011
PG 8
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 740YC
UT WOS:000288829300002
PM 21485399
ER
PT J
AU Sulkowski, CM
Gilkey, KM
Lewandowski, BE
Samorezov, S
Myers, JG
AF Sulkowski, Christina M.
Gilkey, Kelly M.
Lewandowski, Beth E.
Samorezov, Sergey
Myers, Jerry G., Jr.
TI An Extravehicular Suit Impact Load Attenuation Study to Improve
Astronaut Bone Fracture Prediction
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE non-conformal fit; side fall; impact load to hip; space exploration
missions; bone mineral density
ID LONG-DURATION SPACEFLIGHT; FORCE ATTENUATION; HIP; FALL
AB SULKOWSKI CM, GILKEY KM, LEWANDOWSKI BE, SAMOREZOV S, MYERS JR JG. An extravehicular suit impact load attenuation study to improve astronaut bone fracture prediction. Aviat Space Environ Med 2011; 82:455-62. Introduction: Understanding the contributions to the risk of bone fracture during spaceflight is essential for mission success. Methods: A pressurized extravehicular activity (EVA) suit analogue test bed was developed, impact load attenuation data were obtained, and the load at the hip of an astronaut who falls to the side during an EVA was characterized. Offset (representing the gap between the EVA suit and the astronaut's body), impact load magnitude, and EVA suit operating pressure were factors varied in the study. The attenuation data were incorporated into a probabilistic model of bone fracture risk during spaceflight, replacing the previous load attenuation value that was based on commercial hip protector data. Results: Load attenuation was more dependent on offset than on pressurization or load magnitude, especially at small offset values. Load attenuation factors for offsets between 0.1-1.5 cm were 0.69 +/- 0.15, 0.49 +/- 0.22, and 0.35 +/- 0.18 for mean impact forces of 4827, 6400, and 8467 N, respectively. Load attenuation factors for offsets of 2.8-5.3 cm were 0.93 +/- 0.2, 0.94 +/- 0.1, and 0.84 +/- 0.5 for the same mean impact forces. The mean and 95(th) percentile bone fracture risk index predictions were each reduced by 65-83%. The mean and 9.5(th) percentile bone fracture probability predictions were both reduced approximately 20-50%. Discussion: The reduction in uncertainty and improved confidence in bone fracture predictions increased the fidelity and credibility of the fracture risk model and its benefit to mission design and in-flight operational decisions.
C1 [Gilkey, Kelly M.; Lewandowski, Beth E.; Myers, Jerry G., Jr.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Sulkowski, Christina M.] Univ Akron, Akron, OH 44325 USA.
[Samorezov, Sergey] Lerner Res Inst, Cleveland Clin, Cleveland, OH 44106 USA.
RP Lewandowski, BE (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA.
EM beth.e.lewandowski@nasa.gov
FU NASA Johnson Space Center (JSC) Human Research Program (HRP) Office and
the NASA JSC EVA Project Office; National Space Biomedical Research
Institute; Baylor College of Medicine; NASA
FX The authors of this study acknowledge the NASA Johnson Space Center
(JSC) Human Research Program (HRP) Office and the NASA JSC EVA Project
Office for their support of this investigation, especially Shane
McFarland for his professional consultation on the EVA suit. NASA Glenn
Research Center HRP personnel, DeVon Griffin and Gail Perusek, are
appreciated for their supporting role as project managers and technical
reviewers. The investigation team expresses gratitude to Jim King, Dan
Gedeon, and Harkirat Sohi for their technical assistance with the test
operations. The National Space Biomedical Research Institute, Baylor
College of Medicine, and NASA LERCIP programs are also thanked for their
support.
NR 16
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U1 2
U2 7
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD APR
PY 2011
VL 82
IS 4
BP 455
EP 462
DI 10.3357/ASEM.2855.2011
PG 8
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 740YC
UT WOS:000288829300007
PM 21485404
ER
PT J
AU Peters, BT
Miller, CA
Brady, RA
Richards, JT
Mulavara, AP
Bloomberg, JJ
AF Peters, Brian T.
Miller, Chris A.
Brady, Rachel A.
Richards, Jason T.
Mulavara, Ajitkumar P.
Bloomberg, Jacob J.
TI Dynamic Visual Acuity During Walking After Long-Duration Spaceflight
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE spaceflight; human locomotion; dynamic visual acuity; vestibulo-ocular
reflex; adaptation
ID VESTIBULAR HYPOFUNCTION; RESPONSES; RECOVERY
AB PETERS BT, MILLER CA, BRADY RA, RICHARDS JT, MULAVARA AP, BLOOMBERG JJ. Dynamic visual acuity during walking after long-duration spaceflight. Aviat Space Environ Med 2011; 82:463-6.
Astronauts experience alterations in gaze control as a result of adaptive changes in eye-head coordination produced by micro-gravity exposure. This may lead to potential changes in postflight visual acuity during head and body motion. Methods: We gathered dynamic visual acuity (DVA) data from 14 astronauts and cosmonauts after long-duration (similar to 6 mo) stays in space. Walking was used to induce self-motion and visual acuity was determined by sequentially presenting Landolt ring optotypes on a computer display placed 4 m in front of subjects. Acuity assessments were made while seated (static condition) and walking (dynamic condition) at 6.4 km . 1171 on a motorized treadmill. In each condition, a psychophysical threshold detection algorithm minimized the required number of optotype presentations by maximizing the amount displayed around the subject's acuity threshold. The difference between static and dynamic acuity measures provided a metric of change in the subjects' ability to maintain gaze fixation on the visual target while walking. Results: A decrement in postflight visual acuity during walking was found. A mean dynamic acuity decrement of approximately 0.75 eye-chart lines was observed 1 d after returning from space. The population mean showed a consistent improvement in DVA performance during the first postflight week. Discussion: The recovery curves for individual subjects did not necessarily follow a pattern of continuous improvement with each passing day. When adjusted for previous long-duration flight experience, the population mean showed an unexpected DVA reduction in the re-adaptation curve that is similar to recovery patterns observed in prism adaptation studies.
C1 [Peters, Brian T.; Miller, Chris A.; Brady, Rachel A.; Richards, Jason T.] Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA.
[Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA.
[Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA.
RP Peters, BT (reprint author), Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA.
EM brian.peters-1@nasa.gov
FU NASA [E120]; National Space Biomedical Research Institute through NASA
[NCC 9-58]
FX This work was supported by NASA (Experiment E120) and the National Space
Biomedical Research Institute through NASA NCC 9-58.
NR 15
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PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD APR
PY 2011
VL 82
IS 4
BP 463
EP 466
DI 10.3357/ASEM.2928.2011
PG 4
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 740YC
UT WOS:000288829300008
PM 21485405
ER
PT J
AU Thornton, WE
AF Thornton, William E.
TI A Rationale for Space Motion Sickness
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Editorial Material
DE motion sickness
ID INNERVATING OTOLITH ORGANS; SQUIRREL-MONKEY; PHYSIOLOGY
AB THORNTON WE. A rationale for space motion sickness. Aviat Space Environ Med 2011; 82:467-8.
Space motion sickness (SMS) still remains a problematic nuisance for a majority of fliers during their first 1 to 3 clays in space and is an enigma to all concerned after almost half a century of spaceflight and extensive ground and in-flight studies. There is no known etiology consistent with observed signs and symptoms, and attempts to produce pre- and in-flight countermeasures have largely failed. Some medications for motion sickness (MS) have been partially effective, but must be used with caution due to their side effects. A hypothesis regarding SMS that is consistent with current knowledge of vestibular physiology and with observed and measured phenomena during SMS is presented.
C1 NASA, Boerne, TX 78015 USA.
RP Thornton, WE (reprint author), NASA, 7640 Pimlico Lane, Boerne, TX 78015 USA.
EM jwthornt@msn.com
NR 10
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U1 0
U2 5
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD APR
PY 2011
VL 82
IS 4
BP 467
EP 468
DI 10.3357/ASEM.2907.2011
PG 2
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 740YC
UT WOS:000288829300009
PM 21485406
ER
PT J
AU Vanderploeg, J
Campbell, M
Antunano, M
Bagian, J
Bopp, E
Carminati, G
Charles, J
Clague, R
Clark, J
Gedmark, J
Jennings, R
Masten, D
McCormick, M
McDonald, V
McGinnis, P
Michaud, V
Murray, M
Myers, KJ
Parazynski, S
Richard, E
Scheuring, R
Searfoss, R
Snyder, Q
Stepanek, J
Stern, A
Virre, E
Wagner, E
AF Vanderploeg, James
Campbell, Mark
Antunano, Melchor
Bagian, James
Bopp, Eugenia
Carminati, Giugi
Charles, John
Clague, Randall
Clark, Jonathan
Gedmark, John
Jennings, Richard
Masten, David
McCormick, Molly
McDonald, Vernon
McGinnis, Patrick
Michaud, Vincent
Murray, Michelle
Myers, K. Jeffrey
Parazynski, Scott
Richard, Elizabeth
Scheuring, Richard
Searfoss, Richard
Snyder, Quay
Stepanek, Jan
Stern, Alan
Virre, Erik
Wagner, Erika
CA Aerosp Med Assoc
TI Suborbital Commercial Spaceflight Crewmember Medical Issues
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE acceleration; medical certification; neurovestibular dysfunction;
push-pull effect; radiation; weightlessness
ID CENTRAL VENOUS-PRESSURE; SPACE; GZ
AB AEROSPACE MEDICAL ASSOCIATION COMMERCIAL SPACEFLIGHT WORKING GROUP. Position paper: suborbital commercial spaceflight crewmember medical issues. Aviat Space Environ Med 2011; 82:475-84.
As directed by the Council of the Aerospace Medical Association, the Commercial Spaceflight Working Group has developed the following position paper concerning medical issues for commercial suborbital spaceflight crewmembers. This position paper has been approved by the AsMA Council to become a policy of the AsMA.
C1 [Vanderploeg, James] UTMB, Galveston, TX USA.
[Campbell, Mark; Antunano, Melchor] FAA CAMI, Oklahoma City, OK USA.
[Bagian, James] Vet Adm, Northville, MI USA.
[Bopp, Eugenia; McDonald, Vernon; Parazynski, Scott; Richard, Elizabeth] Wyle, Houston, TX USA.
[Carminati, Giugi] Weil Gotshal & Manges, Washington, DC USA.
[Charles, John; Michaud, Vincent; Scheuring, Richard] NASA, Houston, TX USA.
[Clague, Randall; Searfoss, Richard] XCOR, Mojave, CA USA.
[Clark, Jonathan] NSBRI, Houston, TX USA.
[Gedmark, John] Personal Spaceflight Federat, Washington, DC USA.
[Jennings, Richard] UTMB, Galveston, TX USA.
[Masten, David] Masten Space Syst, Mojave, CA USA.
[McCormick, Molly] Orbital Outfitters, Washington, DC USA.
[McGinnis, Patrick] UTMSH, Friendswood, TX USA.
[Murray, Michelle] FAA AST, Washington, DC USA.
[Myers, K. Jeffrey] CHS Med, Merritt Isl, FL USA.
[Stepanek, Jan] Mayo Clin, Scottsdale, AZ USA.
[Snyder, Quay] ALPA, Englewood, CO USA.
[Stern, Alan] SW Res Inst, San Antonio, TX USA.
[Virre, Erik] UCD, Davis, CA USA.
[Wagner, Erika] MIT, Cambridge, MA 02139 USA.
RP Vanderploeg, J (reprint author), UTMB, Galveston, TX USA.
OI Clark, Jonathan/0000-0002-1162-1238
NR 35
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U1 0
U2 4
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD APR
PY 2011
VL 82
IS 4
BP 475
EP 484
DI 10.3357/ASEM.3015.2011
PG 10
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 740YC
UT WOS:000288829300011
ER
PT J
AU Li, WQ
Beard, BL
Johnson, CM
AF Li, Weiqiang
Beard, Brian L.
Johnson, Clark M.
TI Exchange and fractionation of Mg isotopes between epsomite and saturated
MgSO4 solution
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID LOW-TEMPERATURES; MAGNESIUM; EQUILIBRIUM; MECHANISMS; CARBONATE; WATER;
CRYSTALLIZATION; CALIBRATION; MINERALS; CALCITE
AB The equilibrium Mg isotope fractionation factor between epsomite and aqueous MgSO4 solution has been measured using the three isotope method in recrystallization experiments conducted at 7, 20, and 40 degrees C. Complete or near-complete isotopic exchange was achieved within 14 days in all experiments. The Mg isotope exchange rate between epsomite and MgSO4 solution is dependent on the temperature, epsomite seed crystal grain size, and experimental agitation method. The Mg isotope fractionation factors (Delta Mg-26(eps-sol)) at 7, 20, and 40 degrees C are 0.63 +/- 0.07 parts per thousand, 0.58 +/- 0.16 parts per thousand, and 0.56 +/- 0.03 parts per thousand, respectively. These values are indistinguishable within error, indicating that the Mg isotope composition of epsomite is relatively insensitive to temperature. The magnitude of the isotope fractionation factor (Delta Mg-26(eps-sol) = ca. 0.6 parts per thousand 7 and 40 degrees C) indicates that significant Mg isotope variations can be produced in evaporite sequences, and Mg isotopes may therefore, constrain the degree of closed-system behavior, paleo-humidity, and hydrological history of evaporative environments. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Li, Weiqiang] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
NASA Astrobiol Inst, Washington, DC USA.
RP Li, WQ (reprint author), Univ Wisconsin, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA.
EM liweiq@gmail.com
RI Li, Weiqiang/D-2975-2011
OI Li, Weiqiang/0000-0003-2648-7630
FU NASA Astrobiology Institute
FX Dr. Andrew Czaja helped in SEM analysis; Dr. Hiromi Konishi, and Mr.
Fangfu Zhang provided assists in XRD analysis. We thank Dr. Max Coleman
for helpful discussions. The paper benefited from constructive comments
of E. Tipper, N. Vigier, and an anonymous reviewer, as well as editorial
comments by AE M. Rehkamper. This study was supported by the NASA
Astrobiology Institute.
NR 58
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U1 1
U2 27
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 1
PY 2011
VL 75
IS 7
BP 1814
EP 1828
DI 10.1016/j.gca.2011.01.023
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 737TD
UT WOS:000288590200010
ER
PT J
AU Valdivia-Silva, JE
Navarro-Gonzalez, R
Ortega-Gutierrez, F
Fletcher, LE
Perez-Montano, S
Condori-Apaza, R
McKay, CP
AF Valdivia-Silva, Julio E.
Navarro-Gonzalez, Rafael
Ortega-Gutierrez, Fernando
Fletcher, Lauren E.
Perez-Montano, Saul
Condori-Apaza, Renee
McKay, Christopher P.
TI Multidisciplinary approach of the hyperarid desert of Pampas d.e La Joya
in southern Peru as a new Mars-like soil analog
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID ATACAMA DESERT; LABELED RELEASE; NITRATE DEPOSITS; MERIDIANI-PLANUM;
ORGANIC-MATTER; PAST LIFE; CHILE; TEMPERATURE; OPPORTUNITY; AREQUIPA
AB The distribution of living organisms, organic matter, and chemical properties in Mars-like environments on Earth can be used as a model to guide the investigation of possible habitable environments on Mars. This work aims to demonstrate that the place known informally as the "Mar de Cuarzo" (Sea of Quartz) in the Pampas de La Joya desert southern Peru (between 16 S and 17 S latitude), contains soils with characteristics similar to those found on the Martian surface. Using a multidisciplinary approach, we studied the environmental data, geology, organic matter content, oxidant activity, and microbiology of this area. Our data show that (1) Mar de Cuarzo is a hyper arid area with a lower concentration of organic matter than those found in the Mars-like soils from Yungay area (Atacama Desert in Chile), while at the same time having, comparable extreme environmental conditions, and very low levels of microorganisms. (2) The detrital components of the soils come essentially from the Andean volcanic chain and local outcrops of Precambrian gneisses and Cretaceous granitic batholiths. (3) The presence of microclimates, geomorphological features, and the high influence of the "El Nino Southern Oscillation (ENSO)" allowed the formation of exotic and heterogeneous chemical deposits in these soils, including iron oxides, sulfates, and other evaporites. (4) Thermal volatilization in these soils (using methods similar to the Viking and Phoenix instruments) shows high oxidant activity. (5) Labeled release experiment (similar to the Viking instrument) shows high degradation of nutrients added in these soils.
Altogether, the Mar de Cuarzo area in the Pampas de La Joya is an interesting place for astrobiological studies as a new analog to Mars, and for comparative analyses with other hyperarid analogs as Yungay. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Valdivia-Silva, Julio E.; Fletcher, Lauren E.; Condori-Apaza, Renee; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 95054 USA.
[Valdivia-Silva, Julio E.; Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico.
[Ortega-Gutierrez, Fernando] Univ Nacl Autonoma Mexico, Inst Geol, Mexico City 04510, DF, Mexico.
[Perez-Montano, Saul] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Valdivia-Silva, JE (reprint author), NASA, Ames Res Ctr, Div Space Sci, Bldg 245,M-S 245-3, Moffett Field, CA 95054 USA.
EM jvsilva@nucleares.unam.mx
RI Gonzalez, Rafael/D-1748-2009; Valdivia-Silva, Julio/A-2927-2011;
OI Valdivia-Silva, Julio/0000-0002-7061-3756; CONDORI APAZA,
RENEE/0000-0002-1097-5026
FU Universidad Nacional Autonoma de Mexico [IN 107107]; Consejo Nacional de
Ciencia y Tecnologia de Mexico [CONACyT 45810-F]; Posgrado de Ciencias
Biologicas of the Universidad Nacional Autonoma de Mexico; NASA;
National Aeronautics and Space Administration Astrobiology Science and
Technology
FX Funding for this research comes from Grants from the Universidad
Nacional Autonoma de Mexico (IN 107107), Consejo Nacional de Ciencia y
Tecnologia de Mexico (CONACyT 45810-F), fellowship from Posgrado de
Ciencias Biologicas of the Universidad Nacional Autonoma de Mexico,
fellowship from NASA Posdoctoral Program, and by the National
Aeronautics and Space Administration Astrobiology Science and Technology
for Exploring Planets Program. The authors thank to Instituto Geofisico
of the Universidad Nacional San Agustin, Arequipa-Peru, and Mr. Antonio
Ballon for logistical support in the expeditions to the desert.
NR 91
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Z9 6
U1 2
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 1
PY 2011
VL 75
IS 7
BP 1975
EP 1991
DI 10.1016/j.gca.2011.01.017
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 737TD
UT WOS:000288590200020
ER
PT J
AU Zhou, DK
Larar, AM
Liu, X
Smith, WL
Strow, LL
Yang, P
Schlussel, P
Calbet, X
AF Zhou, Daniel K.
Larar, Allen M.
Liu, Xu
Smith, William L.
Strow, L. Larrabee
Yang, Ping
Schluessel, Peter
Calbet, Xavier
TI Global Land Surface Emissivity Retrieved From Satellite Ultraspectral IR
Measurements
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 2nd Workshop on Remote Sensing and Modeling of Surface Properties
CY JUN 09-11, 2009
CL Toulouse, FRANCE
DE Infrared (IR) ultraspectral sounder; inversion; remote sensing; surface
emissivity; temperature
ID RADIATIVE-TRANSFER; VALIDATION; CLOUD; PARAMETERS; CIRRUS
AB Ultraspectral resolution infrared (IR) radiances obtained from nadir observations provide information about the atmosphere, surface, aerosols, and clouds. Surface spectral emissivity (SSE) and surface skin temperature from current and future operational satellites can and will reveal critical information about the Earth's ecosystem and land-surface-type properties, which might be utilized as a means of long-term monitoring of the Earth's environment and global climate change. In this study, fast radiative transfer models applied to the atmosphere under all weather conditions are used for atmospheric profile and surface or cloud parameter retrieval from ultraspectral and/or hyperspectral spaceborne IR soundings. An inversion scheme, dealing with cloudy as well as cloud-free radiances observed with ultraspectral IR sounders, has been developed to simultaneously retrieve atmospheric thermodynamic and surface or cloud microphysical parameters. This inversion scheme has been applied to the Infrared Atmospheric Sounding Interferometer (IASI). Rapidly produced SSE is initially evaluated through quality control checks on the retrievals of other impacted surface and atmospheric parameters. Initial validation of retrieved emissivity spectra is conducted with Namib and Kalahari desert laboratory measurements. Seasonal products of global land SSE and surface skin temperature retrieved with IASI are presented to demonstrate seasonal variation of SSE.
C1 [Zhou, Daniel K.; Larar, Allen M.; Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Smith, William L.] Hampton Univ, Hampton, VA 23668 USA.
[Smith, William L.] Univ Wisconsin, Madison, WI 53706 USA.
[Strow, L. Larrabee] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Yang, Ping] Texas A&M Univ, College Stn, TX 77843 USA.
[Schluessel, Peter; Calbet, Xavier] European Org Exploitat Meteorol Satellites EUMETS, D-64295 Darmstadt, Germany.
RP Zhou, DK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM daniel.k.zhou@nasa.gov
RI Yang, Ping/B-4590-2011
NR 28
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U1 1
U2 17
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 APR
PY 2011
VL 49
IS 4
BP 1277
EP 1290
DI 10.1109/TGRS.2010.2051036
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 740AC
UT WOS:000288762900010
ER
PT J
AU Hulley, GC
Hook, SJ
AF Hulley, Glynn C.
Hook, Simon J.
TI Generating Consistent Land Surface Temperature and Emissivity Products
Between ASTER and MODIS Data for Earth Science Research
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 2nd Workshop on Remote Sensing and Modeling of Surface Properties
CY JUN 09-11, 2009
CL Toulouse, FRANCE
DE ASTER; land surface temperature; MODIS; radiative transfer; spectral
emissivity
ID COVER CHANGE; CLEAR-SKY; ALGORITHM; SEPARATION; RESOLUTION; CONTRAST;
SPECTRA; IMAGES
AB Land surface temperature and emissivity (LST&E) products are generated by the Moderate Resolution Imaging Spectroradiometer (MODIS) and Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) on the National Aeronautics and Space Administration's Terra satellite. These products are generated at different spatial, spectral, and temporal resolutions, resulting in discrepancies between them that are difficult to quantify, compounded by the fact that different retrieval algorithms are used to produce them. The highest spatial resolution MODIS emissivity product currently produced is from the day/night algorithm, which has a spatial resolution of 5 km. The lack of a high-spatial-resolution emissivity product from MODIS limits the usefulness of the data for a variety of applications and limits utilization with higher resolution products such as those from ASTER. This paper aims to address this problem by using the ASTER Temperature Emissivity Separation (TES) algorithm, combined with an improved atmospheric correction method, to generate the LST&E products for MODIS at 1-km spatial resolution and for ASTER in a consistent manner. The rms differences between the ASTER and MODIS emissivities generated from TES over the southwestern U. S. were 0.013 at 8.6 mu m and 0.0096 at 11 mu m, with good correlations of up to 0.83. The validation with laboratory-measured sand samples from the Algodones and Kelso Dunes in CA showed a good agreement in spectral shape and magnitude, with mean emissivity differences in all bands of 0.009 and 0.010 for MODIS and ASTER, respectively. These differences are equivalent to approximately 0.6 K in the LST for a material at 300 K and at 11 mu m.
C1 [Hulley, Glynn C.; Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hulley, GC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM glynn.hulley@jpl.nasa.gov
NR 38
TC 38
Z9 40
U1 3
U2 16
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2011
VL 49
IS 4
BP 1304
EP 1315
DI 10.1109/TGRS.2010.2063034
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 740AC
UT WOS:000288762900012
ER
PT J
AU Feeley, KJ
Silman, MR
Bush, MB
Farfan, W
Cabrera, KG
Malhi, Y
Meir, P
Revilla, NS
Quisiyupanqui, MNR
Saatchi, S
AF Feeley, Kenneth J.
Silman, Miles R.
Bush, Mark B.
Farfan, William
Cabrera, Karina Garcia
Malhi, Yadvinder
Meir, Patrick
Salinas Revilla, Norma
Quisiyupanqui, Mireya Natividad Raurau
Saatchi, Sassan
TI Upslope migration of Andean trees
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Article
DE Andes; climate change; climatic envelope; cloud forest; extinction;
forest plots; global warming; monitoring; Peru; species migration
ID RECENT CLIMATE-CHANGE; AMAZON RAIN-FOREST; BIOTIC ATTRITION; TROPICAL
FORESTS; MOUNTAIN PASSES; EXTINCTION RISK; SEED DISPERSAL; BIODIVERSITY;
TRENDS; SHIFTS
AB Aim
Climate change causes shifts in species distributions, or 'migrations'. Despite the centrality of species distributions to biodiversity conservation, the demonstrated large migration of tropical plant species in response to climate change in the past, and the expected sensitivity of species distributions to modern climate change, no study has tested for modern species migrations in tropical plants. Here we conduct a first test of the hypothesis that increasing temperatures are causing tropical trees to migrate to cooler areas.
Location
Tropical Andes biodiversity hotspot, south-eastern Peru, South America.
Methods
We use data from repeated (2003/04-2007/08) censuses of 14 1-ha forest inventory plots spanning an elevational gradient from 950 to 3400 m in Manu National Park in south-eastern Peru, to characterize changes in the elevational distributions of 38 Andean tree genera. We also analyse changes in the genus-level composition of the inventory plots through time.
Results
We show that most tropical Andean tree genera shifted their mean distributions upslope over the study period and that the mean rate of migration is approximately 2.5-3.5 vertical metres upslope per year. Consistent with upward migrations we also find increasing abundances of tree genera previously distributed at lower elevations in the majority of study plots.
Main conclusions
These findings are in accord with the a priori hypothesis of upward shifts in species ranges due to elevated temperatures, and are potentially the first documented evidence of present-day climate-driven migrations in a tropical plant community. The observed mean rate of change is less than predicted from the temperature increases for the region, possibly due to the influence of changes in moisture or non-climatic factors such as substrate, species interactions, lags in tree community response and/or dispersal limitations. Whatever the cause(s), continued slower-than-expected migration of tropical Andean trees would indicate a limited ability to respond to increased temperatures, which may lead to increased extinction risks with further climate change.
C1 [Feeley, Kenneth J.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA.
[Feeley, Kenneth J.] Fairchild Trop Bot Garden, Ctr Trop Plant Conservat, Coral Gables, FL USA.
[Silman, Miles R.; Farfan, William; Cabrera, Karina Garcia; Quisiyupanqui, Mireya Natividad Raurau] Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA.
[Bush, Mark B.] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA.
[Meir, Patrick] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
[Salinas Revilla, Norma] Univ Nacl San Antonio de Abad Cusco, Herbario Vargas, Cuzco, Peru.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Los Angeles, CA USA.
[Saatchi, Sassan] Univ Calif Los Angeles, Inst Environm, Los Angeles, CA USA.
[Malhi, Yadvinder; Salinas Revilla, Norma] Univ Oxford, Environm Change Inst, Oxford, England.
RP Feeley, KJ (reprint author), Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA.
EM kfeeley@fiu.edu
RI Malhi, Yadvinder/I-4668-2012; Meir, Patrick/J-8344-2012; Farfan-Rios,
William/J-9881-2015; Salinas, Norma/K-8960-2015; Feeley,
Kenneth/A-7631-2009
OI Farfan-Rios, William/0000-0002-3196-0317; Salinas,
Norma/0000-0001-9941-2109; Bush, Mark/0000-0001-6894-8613;
FU Gordon and Betty Moore Foundation (NSF) [DEB-0237684, BCS-0216607]; Blue
Moon Fund; Amazon Conservation Association; FTBG's Center for Tropical
Plant Conservation
FX This paper is a product of the Andes Biodiversity and Ecosystems
Research Group consortium (ABERG; http://www.andesconservation.org). The
data presented here represent an exceptional effort on the part of
botanists and field assistants in Peru, particularly those from the
Universidad Nacional San Antonio de Abad, Cusco, and Luis Imunda
Gonzales. Identifications for the species were aided by more than 20
specialists, and we particularly thank the Universidad Mayor de San
Marcos, the Missouri Botanical Garden, the Field Museum of Natural
History, and the New York Botanical Garden. Support came from the Gordon
and Betty Moore Foundation's Andes to Amazon initiative, NSF DEB-0237684
and NSF BCS-0216607, the Blue Moon Fund, the Amazon Conservation
Association, and the FTBG's Center for Tropical Plant Conservation. We
thank the GBIF and all contributing institutions for making collection
data publicly available. We especially thank INRENA and the personnel of
Manu National Park, Peru, for their gracious help in logistics and
permission to work in the protected area. The Amazon Conservation
Association and the Cock-of-the-Rock Lodge provided logistical support
throughout the project.
NR 43
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Z9 94
U1 18
U2 134
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0305-0270
J9 J BIOGEOGR
JI J. Biogeogr.
PD APR
PY 2011
VL 38
IS 4
BP 783
EP 791
DI 10.1111/j.1365-2699.2010.02444.x
PG 9
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 736AX
UT WOS:000288463000014
ER
PT J
AU Lee, D
Tippur, HV
Jensen, BJ
Bogert, PB
AF Lee, Dongyeon
Tippur, Hareesh V.
Jensen, Brian J.
Bogert, Philip B.
TI Tensile and Fracture Characterization of PETI-5 and IM7/PETI-5
Graphite/Epoxy Composites Under Quasi-Static and Dynamic Loading
Conditions
SO JOURNAL OF ENGINEERING MATERIALS AND TECHNOLOGY-TRANSACTIONS OF THE ASME
LA English
DT Article
DE adhesives; graphite/epoxy composites; fracture; tensile behavior; strain
rate effects; digital image correlation; split-Hopkinson bar
ID IMAGE CORRELATION METHOD; HIGH-SPEED PHOTOGRAPHY; MECHANICS
AB Tensile and fracture responses of the phenylethynyl terminated imide oligomer (PETI-5) are studied. Since this polymer is a candidate aerospace structural adhesive as well as a matrix material in composite systems, neat as well as fiber reinforced forms of PETI-5 are studied under static and dynamic loading conditions. A split-Hopkinson tension bar apparatus is used for performing tensile tests on dogbone specimens. The dynamic fracture tests are carried out using a drop tower in conjunction with 2D image correlation method and high-speed digital photography on edge cracked specimens in three-point bend configuration. A toughened neat epoxy system, Hexcel 3900, is also studied to provide a baseline comparison for neat PETI-5 system. The tensile stress-strain responses show PETI-5 to have excellent mechanical characteristics under quasi-static and dynamic loading conditions when compared with 3900. Fracture behavior of PETI-5 under quasi-static and impact loading conditions also shows superiority relative to 3900. The dynamic fracture behavior of a PETI-5 based graphite fiber reinforced composite, IM7/PETI-5, is also studied and the results are comparatively evaluated relative to the ones corresponding to a more common aerospace composite system, T800/3900-2 graphite/epoxy. Once again, the IM7/PETI-5 system shows excellent fracture performance in terms of dynamic crack initiation and growth behaviors. [DOI: 10.1115/1.4003487]
C1 [Lee, Dongyeon; Tippur, Hareesh V.] Auburn Univ, Dept Mech Engn, Auburn, AL 36830 USA.
[Jensen, Brian J.; Bogert, Philip B.] NASA, Langley Res Ctr, Hampton, VA USA.
RP Tippur, HV (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36830 USA.
EM tippuhv@auburn.edu
FU NASA Langley Research Center under [NNX07AC64A]; Auburn University, AL
FX This research was sponsored by NASA Langley Research Center under a
Grant/Cooperative Agreement (Grant No. NNX07AC64A) with Auburn
University, AL. We would also like to acknowledge the assistance of Mr.
Mark Scott from Hexcel, Inc. for providing the 3900 neat resin plaques.
NR 28
TC 1
Z9 1
U1 1
U2 14
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0094-4289
J9 J ENG MATER-T ASME
JI J. Eng. Mater. Technol.-Trans. ASME
PD APR
PY 2011
VL 133
IS 2
AR 021015
DI 10.1115/1.4003487
PG 11
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 740PR
UT WOS:000288807400015
ER
PT J
AU Makino, A
Nelson, DV
Hill, MR
AF Makino, A.
Nelson, D. V.
Hill, M. R.
TI Hole-Within-a-Hole Method for Determining Residual Stresses
SO JOURNAL OF ENGINEERING MATERIALS AND TECHNOLOGY-TRANSACTIONS OF THE ASME
LA English
DT Article
DE hole drilling; residual stress; optical interference; holographic
interferometry
ID NEUTRON-DIFFRACTION; DRILLING METHOD; DISTRIBUTIONS; CONTOUR
AB The strain gauge rosette hole drilling method is often used for determining residual stresses versus depth to depths on the order of 0.5-1.5 mm. Frequently, it is of interest to find stress profiles to greater depths. To provide such a capability, a new approach is presented. Residual stresses versus depth are found by drilling a small diameter hole incrementally to a depth of half of its diameter. The profile of stresses versus depth is found from changes in surface displacements associated with the stress relief from introducing the hole, observed by optical means. Next, a larger diameter, square-bottomed hole is milled directly over the small hole to a depth equaling that of the smaller diameter hole. The bottom of the larger hole provides a fresh surface for optical observation and incremental drilling of a new small hole. This procedure is repeated until a desired total depth is reached. A computational approach is described for correcting the stresses found from the small holes to account for the perturbation of stresses by the material removed by the larger diameter hole. Results of applying this method to find stresses versus depth in a plate subject to uniaxial bending stress and a plate with biaxial residual stresses that vary from compression to tension through the thickness are shown. [DOI: 10.1115/1.4003496]
C1 [Makino, A.; Nelson, D. V.] Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA.
[Makino, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hill, M. R.] Univ Calif Davis, Dept Mech & Aeronaut Engn, Davis, CA 95616 USA.
RP Nelson, DV (reprint author), Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA.
EM dnelson@stanford.edu
RI Hill, Michael/A-2525-2016
OI Hill, Michael/0000-0002-9168-211X
FU Alcoa Technical Center; Deere & Co. Technical Center
FX We are grateful for support provided by Alcoa Technical Center (M.
Kulak) and Deere & Co. Technical Center (S. Foss) that made this study
possible, as well as the use of experimental facilities (T. Bennett) at
Sandia National Laboratories.
NR 31
TC 1
Z9 1
U1 0
U2 4
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0094-4289
J9 J ENG MATER-T ASME
JI J. Eng. Mater. Technol.-Trans. ASME
PD APR
PY 2011
VL 133
IS 2
AR 021020
DI 10.1115/1.4003496
PG 8
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 740PR
UT WOS:000288807400020
ER
PT J
AU Hilker, T
Gitelson, A
Coops, NC
Hall, FG
Black, TA
AF Hilker, Thomas
Gitelson, Anatoly
Coops, Nicholas C.
Hall, Forrest G.
Black, T. Andrew
TI Tracking plant physiological properties from multi-angular tower-based
remote sensing
SO OECOLOGIA
LA English
DT Article
DE Prosail; Chlorophyll; Carotenoid; Phenology; Radiative transfer;
Light-use efficiency; AMSPEC
ID BIDIRECTIONAL REFLECTANCE MODEL; ESTIMATING AGRONOMIC VARIABLES;
DIFFERENCE VEGETATION INDEX; DECIDUOUS BROADLEAF FOREST; LEAF
CHLOROPHYLL CONTENT; LIGHT-USE EFFICIENCY; SPECTRAL REFLECTANCE;
CARBON-DIOXIDE; SEASONAL-VARIATION; AREA INDEX
AB Imaging spectroscopy is a powerful technique for monitoring the biochemical constituents of vegetation and is critical for understanding the fluxes of carbon and water between the land surface and the atmosphere. However, spectral observations are subject to the sun-observer geometry and canopy structure which impose confounding effects on spectral estimates of leaf pigments. For instance, the sun-observer geometry influences the spectral brightness measured by the sensor. Likewise, when considering pigment distribution at the stand level scale, the pigment content observed from single view angles may not necessarily be representative of stand-level conditions as some constituents vary as a function of the degree of leaf illumination and are therefore not isotropic. As an alternative to mono-angle observations, multi-angular remote sensing can describe the anisotropy of surface reflectance and yield accurate information on canopy structure. These observations can also be used to describe the bi-directional reflectance distribution which then allows the modeling of reflectance independently of the observation geometry. In this paper, we demonstrate a method for estimating pigment contents of chlorophyll and carotenoids continuously over a year from tower-based, multi-angular spectro-radiometer observations. Estimates of chlorophyll and carotenoid content were derived at two flux-tower sites in western Canada. Pigment contents derived from inversion of a CR model (PROSAIL) compared well to those estimated using a semi-analytical approach (r (2) = 0.90 and r (2) = 0.69, P < 0.05 for both sites, respectively). Analysis of the seasonal dynamics indicated that net ecosystem productivity was strongly related to total canopy chlorophyll content at the deciduous site (r (2) = 0.70, P < 0.001), but not at the coniferous site. Similarly, spectral estimates of photosynthetic light-use efficiency showed strong seasonal patterns in the deciduous stand, but not in conifers. We conclude that multi-angular, spectral observations can play a key role in explaining seasonal dynamics of fluxes of carbon and water and provide a valuable addition to flux-tower-based networks.
C1 [Hilker, Thomas; Coops, Nicholas C.] Univ British Columbia, Fac Forest Resources Management, Vancouver, BC V6T 1Z4, Canada.
[Gitelson, Anatoly] Univ Nebraska Lincoln, Sch Nat Resources, Lincoln, NE 68583 USA.
[Hall, Forrest G.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Hall, Forrest G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Black, T. Andrew] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada.
RP Hilker, T (reprint author), Univ British Columbia, Fac Forest Resources Management, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada.
EM thomas.hilker@ubc.ca
RI Gitelson, Anatoly/G-3452-2012; Coops, Nicholas/J-1543-2012
OI Coops, Nicholas/0000-0002-0151-9037
FU Canadian Carbon Program; Natural Sciences and Engineering Research
Council of Canada (NSERC); BIOCAP; NSERC-Accelerator grant
FX Thank you to Zoran Nesic, Dominic Lessard, Andrew Hum and Rick Ketler
from UBC Faculty of Land and Food Systems (LFS) for their assistance in
technical design, installation, and maintenance of AMSPEC II. This
research is partially funded by the Canadian Carbon Program, the Natural
Sciences and Engineering Research Council of Canada (NSERC) and BIOCAP,
and an NSERC-Accelerator grant to Dr. Coops.
NR 70
TC 26
Z9 28
U1 0
U2 33
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
EI 1432-1939
J9 OECOLOGIA
JI Oecologia
PD APR
PY 2011
VL 165
IS 4
BP 865
EP 876
DI 10.1007/s00442-010-1901-0
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA 735EW
UT WOS:000288397200005
PM 21221647
ER
PT J
AU Parente, M
Makarewicz, HD
Bishop, JL
AF Parente, Mario
Makarewicz, Heather D.
Bishop, Janice L.
TI Decomposition of mineral absorption bands using nonlinear least squares
curve fitting: Application to Martian meteorites and CRISM data
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Curve fitting; Gaussian modeling; Remote sensing; VNIR reflectance
spectroscopy; Meteorites; Mars
ID INFRARED SPECTRAL REFLECTANCE; MODIFIED GAUSSIAN MODEL; PYROXENE
MIXTURES; QUANTITATIVE-ANALYSIS; JUVENTAE CHASMA; IRON-OXIDES; MARS;
SPECTROSCOPY; OLIVINE; REGION
AB This study advances curve-fitting modeling of absorption bands of reflectance spectra and applies this new model to spectra of Martian meteorites ALH 84001 and EETA 79001 and data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM). This study also details a recently introduced automated parameter initialization technique. We assess the performance of this automated procedure by comparing it to the currently available initialization method and perform a sensitivity analysis of the fit results to variation in initial guesses. We explore the issues related to the removal of the continuum, offer guidelines for continuum removal when modeling the absorptions and explore different continuum-removal techniques. We further evaluate the suitability of curve fitting techniques using Gaussians/Modified Gaussians to decompose spectra into individual end-member bands. We show that nonlinear least squares techniques such as the Levenberg-Marquardt algorithm achieve comparable results to the MGM model (Sunshine and Pieters, 1993; Sunshine et al., 1990) for meteorite spectra. Finally we use Gaussian modeling to fit CRISM spectra of pyroxene and olivine-rich terrains on Mars. Analysis of CRISM spectra of two regions show that the pyroxene-dominated rock spectra measured at Juventae Chasma were modeled well with low Ca pyroxene, while the pyroxene-rich spectra acquired at Libya Montes required both low-Ca and high-Ca pyroxene for a good fit. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Parente, Mario] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Parente, Mario; Makarewicz, Heather D.; Bishop, Janice L.] NASA, SETI Inst, Ames Res Ctr, Mountain View, CA 94043 USA.
[Makarewicz, Heather D.] Univ Kansas, Lawrence, KS 66045 USA.
RP Parente, M (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA.
EM Mario_Parente@brown.edu; hmakarew@gmail.com; jbishop@seti.org
FU National Science Foundation Office of Polar Programs; MRO/CRISM team;
MDAP program; MFR program
FX We would like to express our thanks to the MRO/CRISM team for all the
data collection and science. Thanks are also due to T. Hiroi of RELAB, a
multi-user facility at the Brown University supported by NASA's
Planetary Geology and Geophysics program for his assistance with the
spectral measurements. We are grateful to J. Sunshine for helpful
discussions of the MGM technique, to V. Hamilton, T. Roush, and W.
Farrand for helpful editorial comments on an earlier version of this
manuscript, to D. Blake for providing the olivine rock from Spitsbergen,
Norway and to R. Kontak for her detailed editorial help. We thank the
Antarctic Meteorite Working Group for providing the meteorite chips and
the Smithsonian Museum for providing the meteorite powders, as well as
the National Science Foundation Office of Polar Programs for funding the
Antarctic Search for Meteorites (ANSMET) activities. Finally, we are
grateful for the support of the MRO/CRISM team and the MDAP and MFR
programs for the funding to make this research possible.
NR 89
TC 14
Z9 15
U1 1
U2 12
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 APR
PY 2011
VL 59
IS 5-6
BP 423
EP 442
DI 10.1016/j.pss.2011.01.009
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737PT
UT WOS:000288581400007
ER
PT J
AU Alonso-Perez, S
Cuevas, E
Perez, C
Querol, X
Baldasano, JM
Draxler, R
De Bustos, JJ
AF Alonso-Perez, S.
Cuevas, E.
Perez, C.
Querol, X.
Baldasano, J. M.
Draxler, R.
De Bustos, J. J.
TI Trend changes of African airmass intrusions in the marine boundary layer
over the subtropical Eastern North Atlantic region in winter
SO TELLUS SERIES B-CHEMICAL AND PHYSICAL METEOROLOGY
LA English
DT Article
ID LONG-TERM TREND; SAHARAN DUST; MINERAL DUST; DESERT DUST; OSCILLATION;
VARIABILITY; TRANSPORT; DEPOSITION; DROUGHT; CLIMATE
AB African dust intrusions in the marine mixing layer of the Eastern North Atlantic subtropical region (23.5 degrees N to 35 degrees N) are favoured in winter when the eastern edge of the Azores High covers Southwestern Europe and North Africa. In situ ground pressure observations and reanalysis from National Centers for Environmental Prediction/National Center for Atmospheric Research (NCEP/NCAR) and European Centre for Medium-Range Weather Forecasts (ECMWF) indicate that the Azores High has strengthened and shifted eastward in winter over the last three decades. This is evidenced by the increase over time of the Madrid-Tenerife Index which is defined as the geopotential height anomaly difference at 1000 mb between Tenerife (28.5 degrees N; 16.3 degrees W) and Madrid (40.5 degrees N; 3.5 degrees W) in winter and of the African Index which is defined as the residence time over Africa of air mass trajectories entering the subtropical Eastern North Atlantic Ocean. Barcelona Supercomputing Center/Dust Regional Atmospheric Model (BSC-DREAM) dust regional model simulations from 1958 to 2006 were performed, assuming that the soil characteristics of dust sources remained unchanged over time. Simulated winter dust concentration levels are well correlated (0.67) with the available background observations for the 1998-2004 period. The model results show a two-fold increase in winter dust concentrations over the 1980-2006 period with respect to the 1958-1979 period, corresponding to the strengthening and eastward shift of the Azores High.
C1 [Alonso-Perez, S.; Cuevas, E.; De Bustos, J. J.] Izana Atmospher Res Ctr AEMET, Santa Cruz De Tenerife 38071, Spain.
[Alonso-Perez, S.; Querol, X.] CSIC, Inst Environm Assessment & Water Res, E-08028 Barcelona, Spain.
[Perez, C.] Columbia Univ, Inst Climate & Soc, NASA, Goddard Inst Space Studies & Int Res,Earth Inst, New York, NY 10025 USA.
[Baldasano, J. M.] Barcelona Supercomp Ctr, Barcelona, Spain.
[Baldasano, J. M.] Univ Politecn Cataluna, E-08028 Barcelona, Spain.
[Draxler, R.] NOAA, Air Resources Lab, Silver Spring, MD 20910 USA.
RP Alonso-Perez, S (reprint author), Izana Atmospher Res Ctr AEMET, C La Marina 20-6A Planta, Santa Cruz De Tenerife 38071, Spain.
EM salonsop@aemet.es
RI Querol, Xavier/E-2800-2014; Alonso Perez, Silvia/M-1035-2014; Cuevas,
Emilio/L-2109-2013;
OI Querol, Xavier/0000-0002-6549-9899; Alonso Perez,
Silvia/0000-0003-0572-6081; Cuevas, Emilio/0000-0003-1843-8302; Perez
Garcia-Pando, Carlos/0000-0002-4456-0697
NR 63
TC 14
Z9 14
U1 0
U2 8
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0280-6509
J9 TELLUS B
JI Tellus Ser. B-Chem. Phys. Meteorol.
PD APR
PY 2011
VL 63
IS 2
BP 255
EP 265
DI 10.1111/j.1600-0889.2010.00524.x
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 736TG
UT WOS:000288516400008
ER
PT J
AU Canan, JW
Pace, S
AF Canan, James W.
Pace, Scott
TI Conversations with Scott Pace
SO AEROSPACE AMERICA
LA English
DT Editorial Material
C1 [Pace, Scott] George Washington Univ, Elliott Sch Int Affairs, Washington, DC 20052 USA.
[Pace, Scott] NASA, Washington, DC USA.
[Pace, Scott] NASAs Off Space Operat, Washington, DC USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0740-722X
J9 AEROSPACE AM
JI Aerosp. Am.
PD APR
PY 2011
VL 49
IS 4
BP 14
EP 17
PG 4
WC Engineering, Aerospace
SC Engineering
GA 981HV
UT WOS:000306958500008
ER
PT J
AU Goldberg, M
Ohring, G
Butler, J
Cao, C
Datla, R
Doelling, D
Gartner, V
Hewison, T
Iacovazzi, B
Kim, D
Kurino, T
Lafeuille, J
Minnis, P
Renaut, D
Schmetz, J
Tobin, D
Wang, L
Weng, F
Wu, X
Yu, F
Zhang, P
Zhu, T
AF Goldberg, M.
Ohring, G.
Butler, J.
Cao, C.
Datla, R.
Doelling, D.
Gaertner, V.
Hewison, T.
Iacovazzi, B.
Kim, D.
Kurino, T.
Lafeuille, J.
Minnis, P.
Renaut, D.
Schmetz, J.
Tobin, D.
Wang, L.
Weng, F.
Wu, X.
Yu, F.
Zhang, P.
Zhu, T.
TI THE GLOBAL SPACE-BASED INTER-CALIBRATION SYSTEM
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID METEOROLOGICAL SATELLITE IMAGERS; RAPID CALIBRATION; INFRARED CHANNELS;
INTERCALIBRATION; WINDOW; WATER
C1 [Goldberg, M.; Ohring, G.; Cao, C.; Iacovazzi, B.; Wang, L.; Weng, F.; Wu, X.; Yu, F.; Zhu, T.] NOAA NESDIS, Camp Springs, MD 20746 USA.
[Butler, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Datla, R.] NIST, Gaithersburg, MD 20899 USA.
[Doelling, D.; Minnis, P.] NASA, LARC, Hampton, VA USA.
[Gaertner, V.] European Space Agcy, Darmstadt, Germany.
[Kim, D.] Korea Meteorol Adm, Seoul, South Korea.
[Kurino, T.] Japan Meteorol Agcy, Tokyo, Japan.
[Lafeuille, J.] WMO, Geneva, Switzerland.
[Renaut, D.] Ctr Natl Etud Spatiales, Paris, France.
[Hewison, T.; Schmetz, J.] European Org Exploitat Meteorol Satellites, Darmstadt, Germany.
[Tobin, D.] Univ Wisconsin, Madison, WI USA.
[Zhang, P.] China Meteorol Adm, Beijing, Peoples R China.
RP Goldberg, M (reprint author), NOAA NESDIS, Room 711,5200 Auth Rd, Camp Springs, MD 20746 USA.
EM mitch.goldberg@noaa.gov
RI Wang, Likun/B-7524-2008; Cao, Changyong/F-5578-2010; Ohring,
George/F-5616-2010; Goldberg, Mitch/F-5589-2010; Yu,
Fangfang/E-7942-2011; Butler, James/D-4188-2013; Wu,
Xiangqian/F-5634-2010; Richards, Amber/K-8203-2015; Minnis,
Patrick/G-1902-2010; Weng, Fuzhong/F-5633-2010
OI Hewison, Tim/0000-0002-7845-5107; Wang, Likun/0000-0001-5646-9746; Yu,
Fangfang/0000-0001-8343-0863; Wu, Xiangqian/0000-0002-7804-5650; Minnis,
Patrick/0000-0002-4733-6148; Weng, Fuzhong/0000-0003-0150-2179
NR 20
TC 70
Z9 70
U1 2
U2 14
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD APR
PY 2011
VL 92
IS 4
BP 467
EP 475
DI 10.1175/2010BAMS2967.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 773QT
UT WOS:000291323900005
ER
PT J
AU Jiao, Z
Woodcock, C
Schaaf, CB
Tan, B
Liu, JC
Gao, F
Strahler, A
Li, XW
Wang, JD
AF Jiao, Ziti
Woodcock, Curtis
Schaaf, Crystal B.
Tan, Bin
Liu, Jicheng
Gao, Feng
Strahler, Alan
Li, Xiaowen
Wang, Jindi
TI Improving MODIS land cover classification by combining MODIS spectral
and angular signatures in a Canadian boreal forest
SO CANADIAN JOURNAL OF REMOTE SENSING
LA English
DT Article
ID REMOTELY-SENSED DATA; BIDIRECTIONAL REFLECTANCE MODEL; HYPERSPECTRAL
BRDF DATA; ACCURACY ASSESSMENT; SPATIAL-RESOLUTION; CHARACTERISTICS
DATABASE; DECISION TREES; EOS-MODIS; SURFACE; ALBEDO
AB This study explores the use of reflectance anisotropy as described by the Bidirectional Reflectance Distribution Function (BRDF) as an additional source of information to improve land surface classification accuracies in a Canadian boreal forest region through the use of a decision tree classifier (C4.5). This effort primarily uses a daily rolling version of the operational algorithm developed for Direct Broadcast to generate 500 m 16-day daily rolling data sets in the study region. Descriptive statistic and statistically rigorous techniques are used to assess classification accuracies based on confusion matrices and a 10-fold cross-validation method. The results show that the inclusion of additional 7-band model anisotropic parameter group (volumetric (VOL) plus geometric (GEO)) with spectral feature group (nadir BRDF-adjusted reflectance (NABR) plus Enhanced Vegetation Index (EVI)) is most useful in classification, increasing overall accuracies by 5.68%. The most improvements of per-class accuracies are seen for Wetland shrub class with user's and producer's accuracies increasing by up to 17.7% and 11.3%, respectively. Increases on the order of 5% to 15% are encountered for the classes of Wetland herb, Wetland tree, Coniferous dense, and Coniferous open with no detriments to other candidate classes. The inclusion of the 2-band BRDF shape indicator group in the classification is, however, not as useful as inclusion of the 7-band model anisotropic parameter group in improving the classification accuracies. A further investigation of the classification accuracies regarding reflectance anisotropy for the sampling pixels within each class shows that land cover types that are dominated by geometric-optical scattering type or a mixture of scattering types are relatively difficult to be classified with spectral feature group alone, and the inclusion of additional BRDF features can significantly improve classification accuracies for these land cover types. However, despite their use as ancillary data, this study also confirms that the spectral feature group provided with NBAR and EVI captures the major information content regarding land cover types, exceeding the information content contained in the model anisotropic parameter group provided with the 7-band VOL and GEO parameters of RossThick-LiSparse-Reciprocal (RTLSR) models.
C1 [Jiao, Ziti; Li, Xiaowen] Beijing Normal Univ, Sch Geog, Beijing 100875, Peoples R China.
[Woodcock, Curtis; Schaaf, Crystal B.; Strahler, Alan; Wang, Jindi] Boston Univ, Dept Geog & Environm, Ctr Remote Sensing, Boston, MA 02215 USA.
[Jiao, Ziti; Li, Xiaowen; Wang, Jindi] Beijing Normal Univ, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Tan, Bin; Gao, Feng] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tan, Bin; Gao, Feng] ERT Inc, Greenbelt, MD 20771 USA.
[Liu, Jicheng] NOAA NESDIS, Camp Springs, MD USA.
RP Jiao, Z (reprint author), Beijing Normal Univ, Sch Geog, Beijing 100875, Peoples R China.
EM jiaozt@bnu.edu.cn
RI Tan, Bin/G-1331-2012; Liu, Jicheng/B-4575-2009
FU NSFC [40871193]; Special Foundation for Free Exploration of State
Laboratory of Remote Sensing Science [610ZY-06]; National Basic Research
Program of China (973 program) [2007CB714402]; NASA [NNX08AE94A]
FX This work was partly supported by NSFC contract (40871193), Special
Foundation for Free Exploration of State Laboratory of Remote Sensing
Science (610ZY-06), and National Basic Research Program of China (973
program, contract No. 2007CB714402). Support was also provided by NASA
grant NNX08AE94A. Thanks are due to a number of colleagues for their
help, advice, and encouragement in relation to various aspects of this
paper, in particular Mark Friedl (Geography and Environment Department,
Boston University, USA) and Michael Hill (Earth System Science and
Policy, University of North Dakota, USA). The comments by the anonymous
reviewers are also greatly appreciated.
NR 65
TC 10
Z9 11
U1 0
U2 21
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 APR
PY 2011
VL 37
IS 2
BP 184
EP 203
PG 20
WC Remote Sensing
SC Remote Sensing
GA 958OO
UT WOS:000305249400002
ER
PT J
AU Falvo, MJ
Blatt, M
Jaisen, J
Miller, R
Wood, SJ
Serrador, JM
AF Falvo, Michael J.
Blatt, Melissa
Jaisen, Jessica
Miller, Rebecca
Wood, Scott J.
Serrador, Jorge M.
TI Cerebral Blood Flow Regulation: Role of Otolith Inputs
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Experimental Biology Meeting 2011
CY APR 09-13, 2011
CL Washington, DC
SP Amer Assoc Anatomists (AAA), Amer Physiolog Soc (APS), Amer Soc Biochem & Mol Biol (ASBMB), Amer Soc Investigat Pathol (ASIP), Amer Soc Nutrit (ASN), Amer Soc Pharmacol & Expt Therapeut (ASPET)
C1 [Falvo, Michael J.; Blatt, Melissa; Jaisen, Jessica; Miller, Rebecca] VA NJ Hlth Care Syst, War Related Illness & Injury Ctr, E Orange, NJ USA.
[Wood, Scott J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Serrador, Jorge M.] Vet Biomed Res Inst, War Related Illness & Injury Ctr, E Orange, NJ USA.
[Serrador, Jorge M.] Harvard Univ, Sch Med, Boston, MA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2011
VL 25
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 032IE
UT WOS:000310708403894
ER
PT J
AU Ploutz-Snyder, L
Ryder, J
Buxton, R
Redd, E
Scott-Pandorf, M
Hackney, K
Fiedler, J
Ploutz-Snyder, R
Bloomberg, J
AF Ploutz-Snyder, Lori
Ryder, Jeff
Buxton, Roxanne
Redd, Elizabeth
Scott-Pandorf, Melissa
Hackney, Kyle
Fiedler, James
Ploutz-Snyder, Robert
Bloomberg, Jacob
TI Novel analog for muscle deconditioning
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Experimental Biology Meeting 2011
CY APR 09-13, 2011
CL Washington, DC
SP Amer Assoc Anatomists (AAA), Amer Physiolog Soc (APS), Amer Soc Biochem & Mol Biol (ASBMB), Amer Soc Investigat Pathol (ASIP), Amer Soc Nutrit (ASN), Amer Soc Pharmacol & Expt Therapeut (ASPET)
C1 [Ploutz-Snyder, Lori; Ryder, Jeff; Fiedler, James; Ploutz-Snyder, Robert] Univ Space Res Assoc, Houston, TX USA.
[Buxton, Roxanne; Redd, Elizabeth] Univ Houston, Houston, TX USA.
[Scott-Pandorf, Melissa] Wyle Integrated Sci & Engn Grp, Houston, TX USA.
[Hackney, Kyle] Syracuse Univ, Houston, TX USA.
[Bloomberg, Jacob] NASA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 1
U2 2
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2011
VL 25
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 032IE
UT WOS:000310708404205
ER
PT J
AU Ravichandran, P
Periyakaruppan, A
Gopikrishnan, R
Biradar, S
Ramesh, V
Hall, JC
Meyyappan, M
Ramesh, G
AF Ravichandran, Prabakaran
Periyakaruppan, Adaikkappan
Gopikrishnan, Ramya
Biradar, Santhoshkumar
Ramesh, Vani
Hall, Joseph C.
Meyyappan, Meyya
Ramesh, Govindarajan
TI Multiwall carbon nanotubes induce apoptosis in rat lung epithelial cells
through activation of caspases
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Experimental Biology Meeting 2011
CY APR 09-13, 2011
CL Washington, DC
SP Amer Assoc Anatomists (AAA), Amer Physiolog Soc (APS), Amer Soc Biochem & Mol Biol (ASBMB), Amer Soc Investigat Pathol (ASIP), Amer Soc Nutrit (ASN), Amer Soc Pharmacol & Expt Therapeut (ASPET)
C1 [Ravichandran, Prabakaran; Gopikrishnan, Ramya; Biradar, Santhoshkumar; Ramesh, Vani; Hall, Joseph C.; Ramesh, Govindarajan] Norfolk State Univ, Norfolk, VA USA.
[Periyakaruppan, Adaikkappan; Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RI Periyakaruppan, Adaikkappan/B-7398-2013
OI Periyakaruppan, Adaikkappan/0000-0002-0395-6564
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2011
VL 25
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 032IE
UT WOS:000310708404618
ER
PT J
AU Shimkus, KL
Zanello, SB
Emami, K
Wu, HL
AF Shimkus, Kevin L.
Zanello, Susana B.
Emami, Kamal
Wu, Honglu
TI Simulated microgravity does not alter myogenesis gene expression in
C2C12 cells
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Experimental Biology Meeting 2011
CY APR 09-13, 2011
CL Washington, DC
SP Amer Assoc Anatomists (AAA), Amer Physiolog Soc (APS), Amer Soc Biochem & Mol Biol (ASBMB), Amer Soc Investigat Pathol (ASIP), Amer Soc Nutrit (ASN), Amer Soc Pharmacol & Expt Therapeut (ASPET)
C1 [Shimkus, Kevin L.] Texas A&M Univ, College Stn, TX USA.
[Zanello, Susana B.] Univ Space Res Assoc, Houston, TX USA.
[Zanello, Susana B.; Emami, Kamal; Wu, Honglu] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Emami, Kamal] Wyle Labs, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2011
VL 25
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 032IE
UT WOS:000310708404204
ER
PT J
AU Lorenzo, CF
AF Lorenzo, Carl F.
TI The Fractional Morphology and Growth Rate of the Nautilus pompilius:
Preliminary Results Based on the R-1-Fractional Trigonometry
SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS
LA English
DT Article
DE fractional calculus; fractional differential equations; fractional
growth rate; fractional spiral; logarithmic spiral; Nautilus
ID SHELL
AB This paper studies the morphology and evolutionary growth of the Nautilus pompilius based on the fractional R-1-trigonometry. Morphological models based on the fractional trigonometry are shown to be superior to those of the commonly assumed logarithmic spiral. The R-1-trigonometric functions further infer fractional differential equations, which, based on power law parametric functions, are used to develop a fractional growth equation modeling evolution from conception to maturity. An important aspect of this work is that it demonstrates a method of determination of the dynamic description of a fractional trigonometrically defined process from its morphological description. [DOI: 10.1115/1.4002343]
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Lorenzo, CF (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM carl.f.lorenzo@nasa.gov
FU NASA Glenn Research Center
FX The author gratefully acknowledges the support of the NASA Glenn
Research Center and the helpful comments of the reviewers.
NR 16
TC 0
Z9 0
U1 0
U2 2
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 1555-1423
J9 J COMPUT NONLIN DYN
JI J. Comput. Nonlinear Dyn.
PD APR
PY 2011
VL 6
IS 2
AR 021004
DI 10.1115/1.4002343
PG 10
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 689XN
UT WOS:000284964300004
ER
PT J
AU Quinet, P
Palmeri, P
Mendoza, C
Bautista, MA
Garcia, J
Witthoeft, MC
Kallman, TR
AF Quinet, P.
Palmeri, P.
Mendoza, C.
Bautista, M. A.
Garcia, J.
Witthoeft, M. C.
Kallman, T. R.
TI Recent advances in the determination of atomic parameters for modeling K
lines in cosmically abundant elements
SO JOURNAL OF ELECTRON SPECTROSCOPY AND RELATED PHENOMENA
LA English
DT Article
DE Atomic processes; K-lines; Radiative rates; Auger rates; Photoionization
ID R-MATRIX APPROACH; AUGER DECAY DATA; SHELL PHOTOIONIZATION; VACANCY
STATES; OPACITY CALCULATIONS; FE-XVII; BREIT; IONS; PHOTOABSORPTION; CA
AB Over the last several years, our group has undertaken a systematic investigation of atomic properties of K-vacancy states in many ions. More precisely, reliable data such as level energies, wavelengths, Einstein A-coefficients, radiative and Auger widths were computed for a large number of ions using three different atomic structure theoretical approaches, i.e. relativistic Hartree-Fock (HER), AUTOSTRUCTURE (AS) and multiconfiguration Dirac-Fock (MCDF) methods. Extensive calculations of photoabsorption and photoionization cross sections were also performed using the Breit-Pauli R-matrix method including the effects of radiative and Auger damping by means of an optical potential. Here, we report on our overall progress concerning N, O, Ne, Mg, Al, Si, S, Ar, Ca, Fe and Ni ions. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Quinet, P.; Palmeri, P.] Univ Mons UMONS, B-7000 Mons, Belgium.
[Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium.
[Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela.
[Bautista, M. A.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Garcia, J.] Catholic Univ Amer, IACS Dept Phys, Washington, DC 20064 USA.
[Garcia, J.; Witthoeft, M. C.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Quinet, P (reprint author), Univ Mons UMONS, B-7000 Mons, Belgium.
EM quinet@umons.ac.be
FU NASA; F.R.S.-FNRS
FX This work was funded in part by the NASA Astronomy and Physics Research
and Analysis Program. The Belgian F.R.S.-FNRS is also acknowledged for
financial support. PP and PQ are respectively Senior Research Associate
and Research Associate of this organization.
NR 28
TC 4
Z9 4
U1 1
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0368-2048
J9 J ELECTRON SPECTROSC
JI J. Electron Spectrosc. Relat. Phenom.
PD APR
PY 2011
VL 184
IS 3-6
SI SI
BP 170
EP 173
DI 10.1016/j.elspec.2010.12.027
PG 4
WC Spectroscopy
SC Spectroscopy
GA 784QN
UT WOS:000292173400018
ER
PT J
AU Smith, MAH
Benner, DC
Predoi-Cross, A
Devi, VM
AF Smith, M. A. H.
Benner, D. Chris
Predoi-Cross, A.
Devi, V. Malathy
TI A multispectrum analysis of the v(4) band of (CH4)-C-13: Widths, shifts,
and line mixing coefficients
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Methane; Widths; Shifts; Line mixing; 13C
ID MOLECULAR SPECTROSCOPIC DATABASE; PRESSURE-INDUCED SHIFTS; Q-BRANCH;
4635 CM(-1); NU(3) BAND; NU(4) BAND; METHANE; CH4; TEMPERATURE
AB Line positions, Lorentz air-broadened half width and air pressure-induced shift coefficients have been measured for nearly 200 transitions in the v(4) band of (CH4)-C-13 from high-resolution spectra recorded with the McMath-Pierce Fourier transform spectrometer. Three room temperature spectra of (CH4)-C-13 used in the previous study of Malathy Devi et al. (Air-broadened Lorentz halfwidths and pressure-induced line shifts in the v(4) band of (CH4)-C-13. Appl. Opt. 1988; 27: 2296-2308) were analyzed together with a large number of additional spectra of self- and air-broadened CH4 recorded at 210-314 K and one room-temperature spectrum of self-broadened (CH4)-C-13. Analyses applying the multispectrum nonlinear least squares fitting technique were performed to retrieve the spectral line parameters. In addition to air-broadened half width and shift coefficients, self-broadened half width and shift coefficients were determined for at least 56 (CH4)-C-13 v(4) transitions. Off-diagonal relaxation matrix element coefficients for air-broadened line mixing were also determined for 28 pairs of P and R transitions in a number off manifolds, and mixing parameters for self-broadening were also determined for some of these pairs. Temperature-dependences of the pressure-induced shift and mixing parameters for the (CH4)-C-13 lines could not be determined from the spectra used in the present analysis, but temperature dependences of the half width coefficients were determined for the strongest transitions. The results of this study are compared with other studies of air- and self-broadened (CH4)-C-13 and 120-14. Published by Elsevier Ltd.
C1 [Smith, M. A. H.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
[Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Predoi-Cross, A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada.
RP Smith, MAH (reprint author), NASA, Sci Directorate, Langley Res Ctr, MS 401A, Hampton, VA 23681 USA.
EM Mary.Ann.H.Smith@nasa.gov
FU National Aeronautics and Space administration; National Sciences and
Engineering Research Council of Canada (NSERC)
FX The authors thank Mike Dulick and Detrick Branston of the National Solar
Observatory for assistance in obtaining the data recorded at Kitt Peak.
The research at the College of William and Mary were performed under
contracts and cooperative agreements with National Aeronautics and Space
administration. A. Predoi-Cross acknowledges the support received from
the National Sciences and Engineering Research Council of Canada
(NSERC). The authors thank NASA's Upper Atmospheres Research Program for
their support of the McMath-Pierce FTS laboratory facility.
NR 36
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U1 2
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2011
VL 112
IS 6
BP 952
EP 968
DI 10.1016/j.jqsrt.2010.11.017
PG 17
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 735ID
UT WOS:000288406600004
ER
PT J
AU Rahman, ZU
Jobson, DJ
Woodell, GA
AF Rahman, Zia-ur
Jobson, Daniel J.
Woodell, Glenn A.
TI Investigating the relationship between image enhancement and image
compression in the context of the multi-scale retinex
SO JOURNAL OF VISUAL COMMUNICATION AND IMAGE REPRESENTATION
LA English
DT Article
DE Image enhancement; Inverting image transforms; Compression; Multi-scale
retinex; End-to-end systems analysis; Image retrieval; Visual
communications channel design; Survey of image compression usage in
space imaging
ID ADVANCED LAND IMAGER; COLOR; PERFORMANCE; ORBITER; MISSION
AB Image enhancement and data compression methods arose from the distinct and largely separate disciplines of image processing and communications respectively, yet both are important components of current and future digital imaging systems technology. Here we examine the relationship of these two components with special emphasis on image enhancement and lossy JPEG image compression. When transmission channel capacity is limited, image/data compression is often performed to increase the data throughput. However, this compression has a significant impact on the quality of the final data that is received. In most cases, image enhancement performed after image compression tends to bring out the artifacts injected into the data due to the compression. However, if image enhancement is performed before image compression, there are two issues that arise: (i) image enhancement typically increases the contrast-amount of observable detail-in an image which leads to poorer compression ratios; and (ii) the radiometric information in the original data is typically irretrievably lost. In this paper we address the impact of image enhancement, specifically that of the multi-scale retinex with color restoration (MSRCR) on image compression, and vice versa. We also look at the impact of compression on recovering original data from enhanced imagery given certain parameters about the enhancement process. In this context, we also develop an inversion process for the MSRCR. (C) 2011 Published by Elsevier Inc.
C1 [Jobson, Daniel J.; Woodell, Glenn A.] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23681 USA.
[Rahman, Zia-ur] Old Dominion Univ, Dept Elect & Comp Engn, Virginia Modeling Anal & Simulat Ctr, Norfolk, VA 23529 USA.
RP Jobson, DJ (reprint author), NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Mailstop 473, Hampton, VA 23681 USA.
EM zrahman@odu.edu; daniel.j.jobson@nasa.gov; glenn.a.woodell@nasa.gov
FU NASA [NNL07AA02A]
FX The authors thank the NASA Aviation Safety Program for the funding which
made this work possible. In particular, Dr. Rahman's work was supported
under NASA cooperative agreement NNL07AA02A.
NR 49
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U1 1
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1047-3203
EI 1095-9076
J9 J VIS COMMUN IMAGE R
JI J. Vis. Commun. Image Represent.
PD APR
PY 2011
VL 22
IS 3
BP 237
EP 250
DI 10.1016/j.jvcir.2010.12.006
PG 14
WC Computer Science, Information Systems; Computer Science, Software
Engineering
SC Computer Science
GA 737SA
UT WOS:000288587300004
ER
PT J
AU Guzman, O
Frew, DJ
Chen, W
AF Guzman, O.
Frew, D. J.
Chen, W.
TI A Kolsky tension bar technique using a hollow incident tube
SO MEASUREMENT SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Kolsky bar; tension test; pulse shaping; dynamic loading; high strain
rate
ID HOPKINSON PRESSURE BAR; COMPRESSION; STRAIN
AB Load control of the incident pulse profiles in compression Kolsky bar experiments has been widely used to subject the specimen to optimal testing conditions. Tension Kolsky bars have been used to determine dynamic material behavior since the 1960s with limited capability to shape the loading pulses due to the pulse-generating mechanisms. We developed a modified Kolsky tension bar where a hollow incident tube is used to carry the incident stress waves. The incident tube also acts as a gas gun barrel that houses the striker for impact. The main advantage of this new design is that the striker impacts on an impact cap of the incident tube. Compression pulse shapers can be attached to the impact cap, thus fully utilizing the predictive compression pulse-shaping capability in tension experiments. Using this new testing technique, the dynamic tensile material behavior for Al 6061-T6511 and TRIP 800 (transformation-induced plasticity) steel has been obtained.
C1 [Frew, D. J.] Dynam Syst & Res Inc, Albuquerque, NM 87110 USA.
[Guzman, O.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Chen, W.] Purdue Univ, W Lafayette, IN 47907 USA.
RP Frew, DJ (reprint author), Dynam Syst & Res Inc, Albuquerque, NM 87110 USA.
EM djfrew@dsr.us.com
NR 20
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Z9 4
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-0233
EI 1361-6501
J9 MEAS SCI TECHNOL
JI Meas. Sci. Technol.
PD APR
PY 2011
VL 22
IS 4
AR 045703
DI 10.1088/0957-0233/22/4/045703
PG 9
WC Engineering, Multidisciplinary; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 735XR
UT WOS:000288454500024
ER
PT J
AU Brozovic, M
Jacobson, RA
Sheppard, SS
AF Brozovic, Marina
Jacobson, Robert A.
Sheppard, Scott S.
TI THE ORBITS OF NEPTUNE'S OUTER SATELLITES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; celestial mechanics; ephemerides; planets and satellites:
general; planets and satellites: individual (Neptune)
ID IRREGULAR SATELLITES; SOLAR-SYSTEM; CAPTURE; DISCOVERY; MOONS;
INCLINATION; PLANETS; TRITON; URANUS
AB In 2009, we used the Subaru telescope to observe all the faint irregular satellites of Neptune for the first time since 2004. These observations extend the data arcs for Halimede, Psamathe, Sao, Laomedeia, and Neso from a few years to nearly a decade. We also report on a search for unknown Neptune satellites in a half-square degree of sky and a limiting magnitude of 26.2 in the R band. No new satellites of Neptune were found. We numerically integrate the orbits for the five irregulars and summarize the results of the orbital fits in terms of the state vectors, post-fit residuals, and mean orbital elements. Sao and Neso are confirmed to be Kozai librators, while Psamathe is a "reverse circulator." Halimede and Laomedeia do not seem to experience any strong resonant effects.
C1 [Brozovic, Marina; Jacobson, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sheppard, Scott S.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Brozovic, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM marina.brozovic@jpl.nasa.gov; raj@jpl.nasa.gov; sheppard@dtm.ciw.edu
FU National Aeronautics and Space Administration
FX The research described here was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. This manuscript was based
partially on data collected at the Subaru telescope, which is operated
by the National Astronomical Observatory of Japan. The authors thank all
of the astronomers who contributed to these orbital calculations with
their measurements.
NR 33
TC 2
Z9 2
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2011
VL 141
IS 4
AR 135
DI 10.1088/0004-6256/141/4/135
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 733IO
UT WOS:000288256600031
ER
PT J
AU Ciardi, DR
von Braun, K
Bryden, G
van Eyken, J
Howell, SB
Kane, SR
Plavchan, P
Ramirez, SV
Stauffer, JR
AF Ciardi, David R.
von Braun, Kaspar
Bryden, Geoff
van Eyken, Julian
Howell, Steve B.
Kane, Stephen R.
Plavchan, Peter
Ramirez, Solange V.
Stauffer, John R.
TI CHARACTERIZING THE VARIABILITY OF STARS WITH EARLY-RELEASE KEPLER DATA
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE stars: statistics; stars: variables: general
ID LOW-MASS STAR; PHOTOMETRIC VARIABILITY; STELLAR VARIABILITY; TARGET
STARS; GIANT STARS; COOL STARS; FIELD; SEARCH; SKY; PLANETS
AB We present a variability analysis of the early-release first quarter of data publicly released by the Kepler project. Using the stellar parameters from the Kepler Input Catalog, we have separated the sample into 129,000 dwarfs and 17,000 giants and further sub-divided the luminosity classes into temperature bins corresponding approximately to the spectral classes A, F, G, K, and M. Utilizing the inherent sampling and time baseline of the public data set (30 minute sampling and 33.5 day baseline), we have explored the variability of the stellar sample. The overall variability rate of the dwarfs is 25% for the entire sample, but can reach 100% for the brightest groups of stars in the sample. G dwarfs are found to be the most stable with a dispersion floor of sigma similar to 0.04 mmag. At the precision of Kepler, >95% of the giant stars are variable with a noise floor of similar to 0.1 mmag, 0.3 mmag, and 10 mmag for the G giants, K giants, and M giants, respectively. The photometric dispersion of the giants is consistent with acoustic variations of the photosphere; the photometrically derived predicted radial velocity distribution for the K giants is in agreement with the measured radial velocity distribution. We have also briefly explored the variability fraction as a function of data set baseline (1-33 days), at the native 30 minute sampling of the public Kepler data. To within the limitations of the data, we find that the overall variability fractions increase as the data set baseline is increased from 1 day to 33 days, in particular for the most variable stars. The lower mass M dwarf, K dwarf, and G dwarf stars increase their variability more significantly than the higher mass F dwarf and A dwarf stars as the time baseline is increased, indicating that the variability of the lower mass stars is mostly characterized by timescales of weeks while the variability of the higher mass stars is mostly characterized by timescales of days. A study of the distribution of the variability as a function of galactic latitude suggests that sources closer to the galactic plane are more variable. This may be the result of sampling differing populations (i.e., ages) as a function of latitude or may be the result of higher background contamination that is inflating the variability fractions at lower latitudes. A comparison of the M dwarf statistics to the variability of 29 known bright M dwarfs indicates that the M dwarfs are primarily variable on timescales of weeks or longer presumably dominated by spots and binarity. On shorter timescales of hours, which are relevant for planetary transit detection, the stars are significantly less variable, with similar to 80% having 12 hr dispersions of 0.5 mmag or less.
C1 [Ciardi, David R.; von Braun, Kaspar; van Eyken, Julian; Kane, Stephen R.; Plavchan, Peter; Ramirez, Solange V.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Bryden, Geoff] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Stauffer, John R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Ciardi, DR (reprint author), CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RI Kane, Stephen/B-4798-2013;
OI Ciardi, David/0000-0002-5741-3047
FU National Aeronautics and Space Administration
FX The authors acknowledge the referee for his or her extremely insightful
and useful comments which made this a better paper. Portions of this
work were performed at the California Institute of Technology under
contract with the National Aeronautics and Space Administration. This
research has made use of the NASA/IPAC Star and Exoplanet Database,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration.
NR 39
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2011
VL 141
IS 4
AR 108
DI 10.1088/0004-6256/141/4/108
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 733IO
UT WOS:000288256600004
ER
PT J
AU Mueller, M
Delbo', M
Hora, JL
Trilling, DE
Bhattacharya, B
Bottke, WF
Chesley, S
Emery, JP
Fazio, G
Harris, AW
Mainzer, A
Mommert, M
Penprase, B
Smith, HA
Spahr, TB
Stansberry, JA
Thomas, CA
AF Mueller, Michael
Delbo', M.
Hora, J. L.
Trilling, D. E.
Bhattacharya, B.
Bottke, W. F.
Chesley, S.
Emery, J. P.
Fazio, G.
Harris, A. W.
Mainzer, A.
Mommert, M.
Penprase, B.
Smith, H. A.
Spahr, T. B.
Stansberry, J. A.
Thomas, C. A.
TI ExploreNEOs. III. PHYSICAL CHARACTERIZATION OF 65 POTENTIAL SPACECRAFT
TARGET ASTEROIDS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; minor planets, asteroids: general;
radiation mechanisms: thermal; space vehicles; surveys
ID NEAR-EARTH ASTEROIDS; 10302 1989 ML; SPECTRAL PROPERTIES; OBJECT SURVEY;
ALBEDOS; TELESCOPE; DIAMETERS; PHOTOMETRY; MAGNITUDE; MISSION
AB Space missions to near-Earth objects (NEOs) are being planned at all major space agencies, and recently a manned mission to an NEO was announced as a NASA goal. Efforts to find and select suitable targets (plus backup targets) are severely hampered by our lack of knowledge of the physical properties of dynamically favorable NEOs. In particular, current mission scenarios tend to favor primitive low-albedo objects. For the vast majority of NEOs, the albedo is unknown. Here we report new constraints on the size and albedo of 65 NEOs with rendezvous Delta nu < 7 km s(-1). Our results are based on thermal-IR flux data obtained in the framework of our ongoing (2009-2011) ExploreNEOs survey using NASA's "Warm-Spitzer" space telescope. As of 2010 July 14, we have results for 293 objects in hand (including the 65 low-Delta nu NEOs presented here); before the end of 2011, we expect to have measured the size and albedo of similar to 700 NEOs (including probably similar to 160 low-Delta nu NEOs). While there are reasons to believe that primitive volatile-rich materials are universally low in albedo, the converse need not be true: the orbital evolution of some dark objects likely has caused them to lose their volatiles by coming too close to the Sun. For all our targets, we give the closest perihelion distance they are likely to have reached (using orbital integrations from Marchi et al. 2009) and corresponding upper limits on the past surface temperature. Low-Delta nu objects for which both albedo and thermal history may suggest a primitive composition include (162998) 2001 SK162, (68372) 2001 PM9, and (100085) 1992 UY4.
C1 [Mueller, Michael; Delbo', M.] Observ Cote Azur, CNRS, UNS, Lab Cassiopee, F-06304 Nice 04, France.
[Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Trilling, D. E.; Thomas, C. A.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA.
[Bhattacharya, B.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA.
[Chesley, S.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Harris, A. W.; Mommert, M.] DLR Inst Planetary Res, D-12489 Berlin, Germany.
[Penprase, B.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Stansberry, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Mueller, M (reprint author), Observ Cote Azur, CNRS, UNS, Lab Cassiopee, BP 4229, F-06304 Nice 04, France.
EM michael.mueller@oca.eu
OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650;
Thomas, Cristina/0000-0003-3091-5757
FU CNRS-INSU; Conseil General des Alpes-Maritimes; ESA
[SSA-NEO-ESA-MEM-017/1]; NASA
FX Michael Mueller gratefully acknowledges the Henri Poincare Fellowship,
which is funded by the CNRS-INSU and the Conseil General des
Alpes-Maritimes. The work of M. M. and M. D. is supported by ESA grant
SSA-NEO-ESA-MEM-017/1. We thank Patrick Michel for helpful discussions.
This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by JPL/Caltech under a contract with NASA.
Support for this work was provided by NASA through an award issued by
JPL/Caltech.
NR 50
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2011
VL 141
IS 4
AR 109
DI 10.1088/0004-6256/141/4/109
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 733IO
UT WOS:000288256600005
ER
PT J
AU Sahai, R
Morris, MR
Villar, GG
AF Sahai, Raghvendra
Morris, Mark R.
Villar, Gregory G.
TI YOUNG PLANETARY NEBULAE: HUBBLE SPACE TELESCOPE IMAGING AND A NEW
MORPHOLOGICAL CLASSIFICATION SYSTEM
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; ISM: jets and outflows; planetary nebulae:
general; stars: AGB and post-AGB; stars: mass-loss; techniques: image
processing
ID MULTIPLE COLLIMATED OUTFLOWS; POINT-SYMMETRIC NEBULAE; PROTOPLANETARY
NEBULAE; PREPLANETARY NEBULA; BIPOLAR NEBULAE; MYCN 18; MAGNETIC-FIELDS;
BINARY-SYSTEMS; SOURCE CATALOG; COAXIAL RINGS
AB Using Hubble Space Telescope images of 119 young planetary nebulae (PNs), most of which have not previously been published, we have devised a comprehensive morphological classification system for these objects. This system generalizes a recently devised system for pre-planetary nebulae, which are the immediate progenitors of PNs. Unlike previous classification studies, we have focused primarily on young PNs rather than all PNs, because the former best show the influences or symmetries imposed on them by the dominant physical processes operating at the first and primary stage of the shaping process. Older PNs develop instabilities, interact with the ambient interstellar medium, and are subject to the passage of photoionization fronts, all of which obscure the underlying symmetries and geometries imposed early on. Our classification system is designed to suffer minimal prejudice regarding the underlying physical causes of the different shapes and structures seen in our PN sample, however, in many cases, physical causes are readily suggested by the geometry, along with the kinematics that have been measured in some systems. Secondary characteristics in our system, such as ansae, indicate the impact of a jet upon a slower-moving, prior wind; a waist is the signature of a strong equatorial concentration of matter, whether it be outflowing or in a bound Keplerian disk, and point symmetry indicates a secular trend, presumably precession, in the orientation of the central driver of a rapid, collimated outflow.
C1 [Sahai, Raghvendra; Villar, Gregory G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morris, Mark R.] Univ Calif Los Angeles, Dept Phys & Astrophys, Div Astron, Los Angeles, CA 90095 USA.
[Villar, Gregory G.] Calif State Polytech Univ Pomona, Dept Phys, Pomona, CA 91768 USA.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
FU NASA [GO 6353.01, 8307.01, 8345.01, 9463.01, 10536.01, 10681.01,
NAS5-26555]; Long Term Space Astrophysics award [NMO710651:
399.20.40.06]
FX We thank Bruce Balick and his students for producing their web catalog
of HST PN images,17 which was helpful in the compilation of
part of the PN sample used in this paper. We thank Noam Soker and Brent
Miszalski for their reading of, and providing helpful comments on, an
earlier version of this paper. R.S.'s contribution to the research
described in this publication was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. Financial support for this work was provided by NASA through
awards (GO 6353.01, 8307.01, 8345.01, 9463.01, 10536.01, 10681.01) from
the Space Telescope Science Institute, operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555 as well as through a Long Term Space Astrophysics award
(NMO710651: 399.20.40.06).
NR 82
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U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2011
VL 141
IS 4
AR 134
DI 10.1088/0004-6256/141/4/134
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 733IO
UT WOS:000288256600030
ER
PT J
AU Batson, CD
Brady, RA
Peters, BT
Ploutz-Snyder, RJ
Mulavara, AP
Cohen, HS
Bloomberg, JJ
AF Batson, Crystal D.
Brady, Rachel A.
Peters, Brian T.
Ploutz-Snyder, Robert J.
Mulavara, Ajitkumar P.
Cohen, Helen S.
Bloomberg, Jacob J.
TI Gait training improves performance in healthy adults exposed to novel
sensory discordant conditions
SO EXPERIMENTAL BRAIN RESEARCH
LA English
DT Article
DE Human locomotion; Unstable support surface; Perturbation; Gait training;
Sensory discordance
ID SPINAL-CORD FUNCTION; LONG-TERM RETENTION; PARKINSONS-DISEASE; TREADMILL
LOCOMOTION; ATTENTIONAL DEMANDS; VIRTUAL ENVIRONMENT; PARAPLEGIC
PATIENTS; VARIABLE PRACTICE; WEIGHT SUPPORT; OPTIC FLOW
AB Recent evidence shows that the ability to adapt to a novel discordant sensorimotor environment can be increased through prior training. We aimed to determine whether gait adaptability could be increased and then retained using a training system comprised of a treadmill placed on a motion base facing a virtual visual scene that provided a variety of sensory challenges that served as training modalities. Ten healthy adults participated in three training sessions during which they walked on a treadmill at 1.1 m/s while receiving discordant support-surface and visual manipulations. Upon completion, participants were presented with a novel sensorimotor challenge designed to test for transfer of adaptive skills. During this test, stride frequency, reaction time, and heart rate data were collected as measures of postural stability, cognitive load, and anxiety, respectively. Compared to 10 untrained controls, trained participants showed enhanced overall performance on the Novel Test, which was administered 20 min after their final training session. Subjects in both groups had greater stride frequency, reaction time, and heart rate when exposed to the new sensory environment; however, these increases were less pronounced in the trained subjects than in the controls. The Novel Test was re-administered to both groups 1 week, 1 month, 3 months, and 6 months later. Trained subjects maintained their level of performance for 6 months. Untrained subjects continued to improve in these measures at each subsequent test session, suggesting that a lasting sensorimotor adaptability training effect can be achieved with very short, repeated exposures to discordant sensory conditions.
C1 [Batson, Crystal D.] MEI Technol Inc, Houston, TX 77058 USA.
[Brady, Rachel A.; Peters, Brian T.] Wyle Integrated Sci & Engn Grp, Houston, TX USA.
[Ploutz-Snyder, Robert J.; Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA.
[Cohen, Helen S.] Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, Houston, TX 77030 USA.
[Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA.
RP Batson, CD (reprint author), MEI Technol Inc, 2525 Bay Area Blvd,Suite 300, Houston, TX 77058 USA.
EM crystal.d.audas@nasa.gov
FU National Space Biomedical Research Institute through NASA NCC [9-58]
FX This work was supported by the National Space Biomedical Research
Institute through NASA NCC 9-58.
NR 36
TC 11
Z9 11
U1 1
U2 4
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0014-4819
J9 EXP BRAIN RES
JI Exp. Brain Res.
PD APR
PY 2011
VL 209
IS 4
BP 515
EP 524
DI 10.1007/s00221-011-2574-6
PG 10
WC Neurosciences
SC Neurosciences & Neurology
GA 733HH
UT WOS:000288253300005
PM 21350808
ER
PT J
AU Baumert, EK
Johnson, WS
Cano, RJ
Jensen, BJ
Weiser, ES
AF Baumert, E. K.
Johnson, W. S.
Cano, R. J.
Jensen, B. J.
Weiser, E. S.
TI Fatigue damage development in new fibre metal laminates made by the
VARTM process
SO FATIGUE & FRACTURE OF ENGINEERING MATERIALS & STRUCTURES
LA English
DT Article
DE fatigue; fibre metal laminate (FML); hybrid composite; tensile
behaviour; vacuum assisted resin transfer moulding (VARTM)
ID GLARE; TOLERANCE
AB This paper investigates the tensile and fatigue properties of a newly developed fibre metal laminate (FML) manufactured using the vacuum assisted resin transfer moulding (VARTM) method. This manufacturing method allows the glass fibre reinforced epoxy and 2024-T3 aluminium FML to be prepared at lower cost than conventionally manufactured FMLs. However, in order for the resin to infiltrate the FML, the metal sheets need to be perforated. These perforation holes act as crack initiators and reduce the FML's performance. Tension and fatigue test results of three different designs are reported and compared to mechanical property predictions. Additionally, single sheet Al alloy specimens were tested in order to analyse the influence of the drilling method.
C1 [Baumert, E. K.; Johnson, W. S.] Georgia Inst Technol, Sch Mat Sci & Engn, Atlanta, GA 30332 USA.
[Cano, R. J.; Jensen, B. J.; Weiser, E. S.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Baumert, EK (reprint author), Georgia Inst Technol, Sch Mat Sci & Engn, Atlanta, GA 30332 USA.
EM eva.baumert@gatech.edu
FU Erich-Becker-Stiftung; Prof. Dr.-Ing. Erich Muller-Stiftung
FX The authors would like to thank the Erich-Becker-Stiftung as well as the
Prof. Dr.-Ing. Erich Muller-Stiftung for their financial support.
NR 25
TC 1
Z9 1
U1 1
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 8756-758X
EI 1460-2695
J9 FATIGUE FRACT ENG M
JI Fatigue Fract. Eng. Mater. Struct.
PD APR
PY 2011
VL 34
IS 4
BP 240
EP 249
DI 10.1111/j.1460-2695.2010.01509.x
PG 10
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 731RS
UT WOS:000288127600002
ER
PT J
AU Currie, D
Dell'Agnello, S
Delle Monache, G
AF Currie, Douglas
Dell'Agnello, Simone
Delle Monache, Giovanni
TI A Lunar Laser Ranging Retroreflector Array for the 21st Century
SO ACTA ASTRONAUTICA
LA English
DT Article; Proceedings Paper
CT 60th International Astronautical Congress
CY OCT 12-16, 2009
CL Daejeon, SOUTH KOREA
DE Lunar Laser Ranging; Retroreflector; Cube Corner Reflector; NASA Lunar
Science Institute; Optical technology; ILN; LLRRA-21; Thermal modeling
AB Over the past 40 years, the Lunar Laser Ranging Program (LLRP) to the Apollo Cube Corner (CCR) Retroreflector Arrays (ALLRRA) [1] has supplied almost all of the significant tests of General Relativity. The LLRP has evaluated the PPN parameters, addressed the possible changes in the gravitational constant and the properties of the self-energy of the gravitational field. In addition, the LLRP has provided significant information on the composition and origin of the moon. This is the only Apollo experiment that is still in operation. Initially the ALLRRAs contributed a negligible fraction of the ranging error budget. Over the decades, the ranging capabilities of the ground stations have improved by more than two orders of magnitude. Now, because of the lunar librations, the existing Apollo retroreflector arrays contribute a significant fraction of the limiting errors in the range measurements.
The University of Maryland, as the Principal Investigator for the original Apollo arrays, is now proposing a new approach to the Lunar Laser Array technology [2]. The investigation of this new technology, with Professor Currie as Principal Investigator, is currently being supported by two NASA programs and by the INFN-LNF in Frascati, Italy. Thus after the proposed installation during the next lunar landing, the new arrays will support ranging observations that are a factor 100 more accurate than the current ALLRRAs.
The new fundamental cosmological physics and the lunar physics [3] that this new Lunar Laser Ranging Retroreflector Array for the 21st Century (LLRRA-21) can provide will be described. In the design of the new array, there are three major challenges: (1) validate the ability to fabricate a CCR of the required specifications, which is significantly beyond the properties of current CCRs, (2) address the thermal and optical effects of the absorption of solar radiation within the CCR, reduce the transfer of heat from the CCR housing and (3) validate an accurate emplacement technique to install the CCR package on the lunar surface. The latter requires a long-term stable relation between the optical center of the array and the deep regolith, that is, below the thermally driven expansion and contraction of the regolith during the lunar day/night cycle. (C) 2010 Published by Elsevier Ltd.
C1 [Currie, Douglas] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Currie, Douglas] NASA, Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA.
[Currie, Douglas; Dell'Agnello, Simone; Delle Monache, Giovanni] Ist Nazl Fis Nucl Lab, Frascati, Italy.
RP Currie, D (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
EM currie@umd.edu; Simone.DellAgnello@lnf.infn.it;
giovanni.dellemonache@lnf.infn.it
NR 18
TC 11
Z9 12
U1 0
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 APR-MAY
PY 2011
VL 68
IS 7-8
BP 667
EP 680
DI 10.1016/j.actaastro.2010.09.001
PG 14
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600004
ER
PT J
AU Kim, MHY
De Angelis, G
Cucinotta, FA
AF Kim, Myung-Hee Y.
De Angelis, Giovanni
Cucinotta, Francis A.
TI Probabilistic assessment of radiation risk for astronauts in space
missions
SO ACTA ASTRONAUTICA
LA English
DT Article; Proceedings Paper
CT 60th International Astronautical Congress
CY OCT 12-16, 2009
CL Daejeon, SOUTH KOREA
DE Probabilistic risk assessment; Solar particle event; Galactic cosmic
radiation; Organ doses
ID SOLAR PARTICLE EVENTS; EXPLORATION MISSIONS; MAGNETIC-FIELD; EXPOSURE;
FREQUENCY; CYCLES; MODEL
AB Accurate estimations of the health risks to astronauts due to space radiation exposure are necessary for future lunar and Mars missions. Space radiation consists of solar particle events (SPEs), comprised largely of medium energy protons (less than several hundred MeV); and galactic cosmic rays (GCR), which include high-energy protons and heavy ions. While the frequency distribution of SPEs depends strongly upon the phase within the solar activity cycle, the individual SPE occurrences themselves are random in nature. A solar modulation model has been developed for the temporal characterization of the GCR environment, which is represented by the deceleration potential, phi. The risk of radiation exposure to astronauts as well as to hardware from SPEs during extravehicular activities (EVAs) or in lightly shielded vehicles is a major concern for radiation protection. To support the probabilistic risk assessment for EVAs, which could be up to 15% of crew time(2) on lunar missions, we estimated the probability of SPE occurrence as a function of solar cycle phase using a non-homogeneous Poisson model [1] to fit the historical database of measurements of protons with energy > 30 MeV, phi(30). The resultant organ doses and dose equivalents, as well as effective whole body doses, for acute and cancer risk estimations are analyzed for a conceptual habitat module and for a lunar rover during space missions of defined durations. This probabilistic approach to radiation risk assessment from SPE and GCR is in support of mission design and operational planning for future manned space exploration missions. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Kim, Myung-Hee Y.] Univ Space Res Assoc, Houston, TX 77058 USA.
[De Angelis, Giovanni] Ist Super Sanita, I-00161 Rome, Italy.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Kim, MHY (reprint author), Univ Space Res Assoc, Houston, TX 77058 USA.
EM myung-hee.y.kim@nasa.gov; giovanni.angelis@cllr.de;
francis.a.cucinotta@nasa.gov
OI Kim, Myung-Hee/0000-0001-5575-6858
NR 42
TC 10
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U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD APR-MAY
PY 2011
VL 68
IS 7-8
BP 747
EP 759
DI 10.1016/j.actaastro.2010.08.035
PG 13
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600014
ER
PT J
AU Arai, T
Lee, K
Stenger, MB
Platts, SH
Meck, JV
Cohen, RJ
AF Arai, Tatsuya
Lee, Kichang
Stenger, Michael B.
Platts, Steven H.
Meck, Janice V.
Cohen, Richard J.
TI Preliminary application of a novel algorithm to monitor changes in
pre-flight total peripheral resistance for prediction of post-flight
orthostatic intolerance in astronauts
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Orthostatic intolerance; Presyncope; Spaceflight; Astronauts; Blood
pressure; Total peripheral resistance
ID CONTINUOUS CARDIAC-OUTPUT; PRESSURE WAVE-FORM; PULSE CONTOUR ANALYSIS;
ARTERIAL-PRESSURE; VASCULAR-RESISTANCE; BED REST; SPACEFLIGHT;
HYPOTENSION; HUMANS; WINDKESSEL
AB Orthostatic intolerance (01) is a significant challenge for astronauts after long-duration spaceflight. Depending on flight duration, 20-80% of astronauts suffer from post-flight OI, which is associated with reduced vascular resistance. This paper introduces a novel algorithm for continuously monitoring changes in total peripheral resistance (TPR) by processing the peripheral arterial blood pressure (ABP). To validate, we applied our novel mathematical algorithm to the pre-flight ABP data previously recorded from twelve astronauts ten days before launch. The TPR changes were calculated by our algorithm and compared with the TPR value estimated using cardiac output/heart rate before and after phenylephrine administration. The astronauts in the post-flight presyncopal group had lower pre-flight TPR changes (1.66 times) than those in the non-presyncopal group (2.15 times). The trend in TPR changes calculated with our algorithm agreed with the TPR trend calculated using measured cardiac output in the previous study. Further data collection and algorithm refinement are needed for pre-flight detection of 01 and monitoring of continuous TPR by analysis of peripheral arterial blood pressure. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Arai, Tatsuya] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA.
[Lee, Kichang; Cohen, Richard J.] MIT, Harvard MIT Div Hlth Sci & Technol, Cambridge, MA 02139 USA.
[Stenger, Michael B.] Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA.
[Platts, Steven H.; Meck, Janice V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Arai, T (reprint author), MIT, Dept Aeronaut & Astronaut, 77 Massachusetts Ave,45 Carleton St,E25-335, Cambridge, MA 02139 USA.
EM tatsuya@mit.edu
FU National Space Biomedical Research Institute
FX This work was partly supported by the National Space Biomedical Research
Institute Summer Internship Program.
NR 33
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U1 0
U2 0
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD APR-MAY
PY 2011
VL 68
IS 7-8
BP 770
EP 777
DI 10.1016/j.actaastro.2010.10.008
PG 8
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600016
ER
PT J
AU Brandon, EJ
Vozoff, M
Kolawa, EA
Studor, GF
Lyons, F
Keller, MW
Beiermann, B
White, SR
Sottos, NR
Curry, MA
Banks, DL
Brocato, R
Zhou, LS
Jung, SY
Jackson, TN
Champaigne, K
AF Brandon, Erik J.
Vozoff, Max
Kolawa, Elizabeth A.
Studor, George F.
Lyons, Frankel
Keller, Michael W.
Beiermann, Brett
White, Scott R.
Sottos, Nancy R.
Curry, Mark A.
Banks, David L.
Brocato, Robert
Zhou, Lisong
Jung, Soyoun
Jackson, Thomas N.
Champaigne, Kevin
TI Structural health management technologies for inflatable/deployable
structures: Integrating sensing and self-healing
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Inflatable structures; Deployable structures; Distributed sensing;
Structural health monitoring; Self-repairing materials
ID INFLATABLE STRUCTURES; TEAR PROPERTIES; SAW DEVICES; COMPOSITE; SENSORS;
LUNAR; ELECTRONICS; CATALYST; RUPTURE; RUBBER
AB Inflatable/deployable structures are under consideration as habitats for future Lunar surface science operations. The use of non-traditional structural materials combined with the need to maintain a safe working environment for extended periods in a harsh environment has led to the consideration of an integrated structural health management system for future habitats, to ensure their integrity. This article describes recent efforts to develop prototype sensing technologies and new self-healing materials that address the unique requirements of habitats comprised mainly of soft goods. A new approach to detecting impact damage is discussed, using addressable flexible capacitive sensing elements and thin film electronics in a matrixed array. Also, the use of passive wireless sensor tags for distributed sensing is discussed, wherein the need for on-board power through batteries or hardwired interconnects is eliminated. Finally, the development of a novel, microencapuslated self-healing elastomer with applications for inflatable/deployable habitats is reviewed. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Brandon, Erik J.; Vozoff, Max; Kolawa, Elizabeth A.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[Studor, George F.; Lyons, Frankel] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Keller, Michael W.; Beiermann, Brett; White, Scott R.; Sottos, Nancy R.] Univ Illinois, Urbana, IL 61801 USA.
[Curry, Mark A.; Banks, David L.] Boeing Phantom Works, Seattle, WA 98124 USA.
[Brocato, Robert] Sandia Natl Labs, Albuquerque, NM 87185 USA.
[Zhou, Lisong; Jung, Soyoun; Jackson, Thomas N.] Penn State Univ, University Pk, PA 16802 USA.
[Champaigne, Kevin] Invocon Inc, Conroe, TX 77385 USA.
RP Brandon, EJ (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM erik.j.brandon@jpl.nasa.gov; Max.Vozoff@spacex.com;
Elizabeth.A.Kolawa@jpl.nasa.gov; george.f.studor@nasa.gov;
frankel.lyons-1@nasa.gov; mwkeller@utulsa.edu; bbeierm2@illinois.edu;
swhite@uiuc.edu; n-sottos@uiuc.edu; mark.a.curry@boeing.com;
david.l.banks@boeing.com; rwbroca@sandia.gov; Lisong_zhou@amat.com;
sxj001@uark.edu; tnj1@psu.edu; champaigne@invocon.com
RI Jackson, Thomas/A-4224-2012; Keller, Michael/B-6853-2008
OI Keller, Michael/0000-0002-6069-0280
FU NASA Exploration and Science Mission Directorate
FX The authors thank Chris Moore of NASA Headquarters and Judith Watson of
NASA Langley Research Center for their guidance and support during this
project, Benny Toomarian, Mohammad Mojarradi and Anil Thakoor of JPL for
helpful discussions and John Frassanito and Associates for the use of
the habitat images. This work was performed by the Jet Propulsion
Laboratory, California Institute of Technology through the support of
the NASA Exploration and Science Mission Directorate.
NR 57
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U1 4
U2 35
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 APR-MAY
PY 2011
VL 68
IS 7-8
BP 883
EP 903
DI 10.1016/j.actaastro.2010.08.016
PG 21
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600026
ER
PT J
AU Kloster, KW
Petropoulos, AE
Longuski, JM
AF Kloster, Kevin W.
Petropoulos, Anastassios E.
Longuski, James M.
TI Europa Orbiter tour design with Io gravity assists
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Europa Orbiter; Tisserand graph; Tour design
AB For a Europa Orbiter mission, the strategy for designing Jovian System tours that include Io flybys differs significantly from schemes developed for previous versions of the mission. Assuming that the closest approach distance of the incoming hyperbola at Jupiter is below the orbit of Io, then an Io gravity assist gives the greatest energy pump-down for the least decrease in perijove radius. Using Io to help capture the spacecraft can increase the savings in Jupiter orbit insertion Delta V over a Ganymede-aided capture. The tour design is guided by Tisserand graphs overlaid with a simple and accurate radiation model so that tours including Io flybys can maintain an acceptable radiation dosage. While Io flybys increase the duration of tours that are ultimately bound for Europa, they offer Delta V savings and greater scientific return, including the possibility of flying through the plume of one of Io's volcanoes. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Kloster, Kevin W.; Longuski, James M.] Purdue Univ, W Lafayette, IN 47907 USA.
[Petropoulos, Anastassios E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kloster, KW (reprint author), Purdue Univ, Armstrong Hall,701 W Stadium Ave, W Lafayette, IN 47907 USA.
EM kkloster@purdue.edu
FU National Aeronautics and Space Administration
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration as part of the Jupiter Europa
Orbiter flagship mission study. The information in this paper is
pre-decisional-for planning and discussion purposes only. The authors
thank Jan Ludwinski, Jon Sims, Nathan Strange, Jennie Johannesen, Brent
Buffington, and Chris Ballard for their guidance and insight throughout
the process of doing this research; Dave Skinner, Chen-Wan Yen, Alfred
Lynam, and Try Lam for their help with software; and Jan Ludwinski,
Karla Clark, Bob Pappalardo, and Rob Lock for their guidance on Europa
science requirements.
NR 22
TC 12
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U1 1
U2 2
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD APR-MAY
PY 2011
VL 68
IS 7-8
BP 931
EP 946
DI 10.1016/j.actaastro.2010.08.041
PG 16
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600029
ER
PT J
AU Quadrelli, MB
Backes, P
Wilkie, WK
Giersch, L
Quijano, U
Keim, J
Scharf, D
Mukherjee, R
Bradford, SC
Mckee, M
AF Quadrelli, Marco B.
Backes, Paul
Wilkie, W. Keats
Giersch, Lou
Quijano, Ubaldo
Keim, Jason
Scharf, Daniel
Mukherjee, Rudranarayan
Bradford, S. Case
McKee, Michael
TI Investigation of phase transition-based tethered systems for small body
sample capture
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Planetary sample capture; Tethered systems; Distributed control;
Adaptive structures; Robotic manipulation; Phase transition; Shape
memory
ID SHAPE-MEMORY
AB This paper summarizes the modeling, simulation, and testing work related to the development of technology to investigate the potential that shape memory actuation has to provide mechanically simple and affordable solutions for delivering assets to a surface and for sample capture and possible return to Earth. We investigate the structural dynamics and controllability aspects of an adaptive beam carrying an end-effector which, by changing material equilibrium phases, is able to actively decouple the end-effector dynamics from the spacecraft dynamics during the surface contact phase. Asset delivery and sample capture and return are at the heart of several emerging potential missions to small bodies, such as asteroids and comets, and to the surface of large bodies, such as Titan. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Quadrelli, Marco B.; Backes, Paul; Wilkie, W. Keats; Giersch, Lou; Quijano, Ubaldo; Keim, Jason; Scharf, Daniel; Mukherjee, Rudranarayan; Bradford, S. Case; McKee, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Quadrelli, MB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 198-326, Pasadena, CA 91109 USA.
EM Marco.B.Quadrelli@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. The first author is very grateful
to the following JPL colleagues for fruitful interactions during the
course of this investigation: Dr. Fred Hadaegh, Dr. David Bayard, and
Dr. Al Cangahuala.
NR 17
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U2 7
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD APR-MAY
PY 2011
VL 68
IS 7-8
BP 947
EP 973
DI 10.1016/j.actaastro.2010.08.040
PG 27
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600030
ER
PT J
AU Singleterry, RC
Blattnig, SR
Clowdsley, MS
Qualls, GD
Sandridge, CA
Simonsen, LC
Slaba, TC
Walker, SA
Badavi, FF
Spangler, JL
Aumann, AR
Zapp, EN
Rutledge, RD
Lee, KT
Norman, RB
Norbury, JW
AF Singleterry, Robert C., Jr.
Blattnig, Steve R.
Clowdsley, Martha S.
Qualls, Garry D.
Sandridge, Chris A.
Simonsen, Lisa C.
Slaba, Tony C.
Walker, Steven A.
Badavi, Francis F.
Spangler, Jan L.
Aumann, Aric R.
Zapp, E. Neal
Rutledge, Robert D.
Lee, Kerry T.
Norman, Ryan B.
Norbury, John W.
TI OLTARIS: On-line tool for the assessment of radiation in space
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Space radiation; Solar particle event; Galactic cosmic rays
ID NUCLEAR FRAGMENTATION MODEL; ADULT VOXEL PHANTOM; PROTECTION DOSIMETRY;
ENERGY DEPOSITION; AIR MODEL; IONIZATION; SITES; IONS
AB OLTARIS (On-Line Tool for the Assessment of Radiation In Space) is a space radiation analysis tool available on the World Wide Web. It can be used to study the effects of space radiation for various spacecraft and mission scenarios involving humans and electronics. The transport is based on the HZETRN transport code and the input nuclear physics model is NUCFRG. This paper describes the tools behind the web interface and the types of inputs required to obtain results. Typical inputs are mission parameters and slab definitions or vehicle thickness distributions. Radiation environments can be chosen by the user. This paper describes these inputs as well as the output response functions including dose, dose equivalent, whole body effective dose equivalent, LET spectra and detector response models. (C) 2010 Published by Elsevier Ltd.
C1 [Singleterry, Robert C., Jr.; Blattnig, Steve R.; Clowdsley, Martha S.; Qualls, Garry D.; Sandridge, Chris A.; Simonsen, Lisa C.; Slaba, Tony C.; Norman, Ryan B.; Norbury, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Walker, Steven A.] Old Dominion Univ, Norfolk, VA 23529 USA.
[Badavi, Francis F.] Christopher Newport Univ, Newport News, VA 23606 USA.
[Spangler, Jan L.] Lockheed Martin Operat Support, Hampton, VA 23681 USA.
[Aumann, Aric R.] Analyt Serv & Mat, Hampton, VA 23681 USA.
[Zapp, E. Neal; Rutledge, Robert D.; Lee, Kerry T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Norbury, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM john.w.norbury@nasa.gov
RI Norman, Ryan/D-5095-2017
OI Norman, Ryan/0000-0002-9103-7225
FU Human Research Program in the Advanced Capabilities Division under the
Exploration Systems Mission Directorate
FX This work was supported by the Human Research Program in the Advanced
Capabilities Division under the Exploration Systems Mission Directorate
and performed by the members of the Design Tool Project in the Space
Radiation Program Element.
NR 58
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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 APR-MAY
PY 2011
VL 68
IS 7-8
BP 1086
EP 1097
DI 10.1016/j.actaastro.2010.09.022
PG 12
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600043
ER
PT J
AU Elliott, J
Alkalai, L
AF Elliott, John
Alkalai, Leon
TI Lunette: A network of lunar landers for in-situ geophysical science
SO ACTA ASTRONAUTICA
LA English
DT Article; Proceedings Paper
CT 60th International Astronautical Congress
CY OCT 12-16, 2009
CL Daejeon, SOUTH KOREA
DE Lunar lander; Network
AB Over the last 3 years, a team at JPL has worked to design a new concept for a small, low cost lander applicable to a variety of in-situ lunar exploration activities. This concept, named Lunette, originated as a design which would exploit potential excess capacity of EELV launches by being compatible with the EELV Secondary Payload Adapter (ESPA). The original Lunette mission concept would have allowed up to six low cost landers to be delivered to a targeted region of the moon, with landings separated by a few km, allowing establishment of a regional network with a single, shared launch. The original concept faced limits in the extent of regional distribution of landing sites since all six landers were dependent on a single solid rocket braking motor. In the last year the Lunette team has focused on a modification of the original ESPA-based concept to a design that would allow launch of multiple individual landers (each with its own braking stage) on a single launch vehicle, where each lander would be capable of independent targeting and landing. With such an implementation, the entire lunar surface could be accessed for establishment of network nodes that could enable high priority geophysical measurements on a scale not seen since Apollo. The present paper discusses the current state of the design of the Lunette geophysical network lander, as well as describing mission design, science operations, and an innovative design solution allowing the lander to take critical data continuously, even over the lunar night, without the need for radioisotope power systems. (C) 2010 Published by Elsevier Ltd.
C1 [Elliott, John; Alkalai, Leon] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Elliott, J (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM jelliott@jpl.nasa.gov
NR 5
TC 6
Z9 6
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 APR-MAY
PY 2011
VL 68
IS 7-8
BP 1201
EP 1207
DI 10.1016/j.actaastro.2010.10.024
PG 7
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600053
ER
PT J
AU Campbell, JF
Brandon, JM
AF Campbell, Joel F.
Brandon, Jay M.
TI Calibration and flight results for the Ares I-X 5-hole probe
SO ACTA ASTRONAUTICA
LA English
DT Article
DE 5-Hole probe; Five-hole probe; Angle of attack; Mach speed;
Aerodynamics; Supersonic flow; Fluid mechanics; CFD; USM 3D; Pressure;
Supersonic; Pressure measurement; Plenum; Data acquisition; Best
estimated trajectory
AB Flight and calibration results are presented for the Ares I-X 5-hole probe. The probe is calibrated by using a combination of wind tunnel, CFD, and other numerical modeling techniques. This is then applied to the probe flight data and comparisons are made between the vanes and 5-hole probe. Using this and other data it is shown the probe was Keywords: corrupted by water rendering that measurement unreliable. Published by Elsevier Ltd.
C1 [Campbell, Joel F.; Brandon, Jay M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Campbell, JF (reprint author), NASA, Langley Res Ctr, MS 488, Hampton, VA 23681 USA.
EM joel.f.campbell@nasa.gov
NR 7
TC 1
Z9 1
U1 1
U2 1
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 APR-MAY
PY 2011
VL 68
IS 7-8
BP 1219
EP 1227
DI 10.1016/j.actaastro.2010.10.020
PG 9
WC Engineering, Aerospace
SC Engineering
GA 727SL
UT WOS:000287821600055
ER
PT J
AU Gray, MA
Stone, RP
McLaughlin, MR
Kellogg, CA
AF Gray, Michael A.
Stone, Robert P.
McLaughlin, Molly R.
Kellogg, Christina A.
TI Microbial consortia of gorgonian corals from the Aleutian islands
SO FEMS MICROBIOLOGY ECOLOGY
LA English
DT Article
DE cold-water coral; deep sea; bacteria; mycoplasma
ID LOPHELIA-PERTUSA SCLERACTINIA; COLD-WATER CORALS; BACTERIAL COMMUNITIES;
SP-NOV.; POCILLOPORA-DAMICORNIS; SPECIES ASSOCIATIONS; GEN. NOV.;
DIVERSITY; DEEP; SEA
AB Gorgonians make up the majority of corals in the Aleutian archipelago and provide critical fish habitat in areas of economically important fisheries. The microbial ecology of the deep-sea gorgonian corals Paragorgea arborea, Plumarella superba, and Cryogorgia koolsae was examined with culture-based and 16S rRNA gene-based techniques. Six coral colonies (two per species) were collected. Samples from all corals were cultured, and clone libraries were constructed from P. superba and C. koolsae. Cultured bacteria were dominated by the Gammaproteobacteria, especially Vibrionaceae, with other phyla comprising < 6% of the isolates. The clone libraries showed dramatically different bacterial communities between corals of the same species collected at different sites, with no clear pattern of conserved bacterial consortia. Two of the clone libraries (one from each coral species) were dominated by Tenericutes, with Alphaproteobacteria dominating the remaining sequences. The other libraries were more diverse and had a more even distribution of bacterial phyla, showing more similarity between genera than within coral species. Here we report the first microbiological characterization of P. arborea, P. superba, and C. koolsae.
C1 [Gray, Michael A.; McLaughlin, Molly R.; Kellogg, Christina A.] US Geol Survey, St Petersburg, FL 33701 USA.
[Stone, Robert P.] Natl Ocean & Atmospher Adm, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK USA.
RP Kellogg, CA (reprint author), US Geol Survey, 600 4th St S, St Petersburg, FL 33701 USA.
EM ckellogg@usgs.gov
OI Kellogg, Christina/0000-0002-6492-9455
FU North Pacific Research Board; National Marine Fisheries Service (Alaska
Fisheries Science Center)
FX The authors especially thank the crew of the RV Velero IV, Delta
Oceanographics, and Helmut Lehnert and Dave Carlile for help in
collecting the study animals. This project was partially funded by the
North Pacific Research Board and National Marine Fisheries Service
(Alaska Fisheries Science Center). Any use of trade names is for
descriptive purposes only and does not imply endorsement by the US
Government.
NR 49
TC 24
Z9 24
U1 2
U2 9
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0168-6496
J9 FEMS MICROBIOL ECOL
JI FEMS Microbiol. Ecol.
PD APR
PY 2011
VL 76
IS 1
BP 109
EP 120
DI 10.1111/j.1574-6941.2010.01033.x
PG 12
WC Microbiology
SC Microbiology
GA 730ZF
UT WOS:000288075400010
PM 21223327
ER
PT J
AU Moffitt, CB
Hossain, F
Adler, RF
Yilmaz, KK
Pierce, HF
AF Moffitt, Caitlin Balthrop
Hossain, Faisal
Adler, Robert F.
Yilmaz, Koray K.
Pierce, Harold F.
TI Validation of a TRMM-based global Flood Detection System in Bangladesh
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Article
DE Satellites; Transboundary flooding; Ungauged basins; Tropical Rainfall
Measuring Mission; Rainfall; Ground validation
ID MEASURING MISSION TRMM; PRECIPITATION PRODUCTS; SATELLITE; BASIN
AB Although the TRMM-based Flood Detection System (FDS) has been in operation in near real-time since 2006, the flood 'detection' capability has been validated mostly against qualitative reports in news papers and other types of media. In this study, a more quantitative validation of the FDS over Bangladesh against in situ measurements is presented. Using measured stream flow and rainfall data, the study analyzed the flood detection capability from space for three very distinct river systems in Bangladesh: (1) Gangesa snowmelt-fed river regulated by upstream India, (2) Brahmaputra - a snow-fed river that is braided, and (3) Meghna - a rain-fed and relatively flashier river. The quantitative assessment showed that the effectiveness of the TRMM-based FDS can vary as a function of season and drainage basin characteristics. Overall, the study showed that the TRMM-based FDS has great potential for flood prone countries like Bangladesh that are faced with tremendous hurdles in transboundary flood management. The system had a high probability of detection overall, but produced increased false alarms during the monsoon period and in regulated basins (Ganges), undermining the credibility of the FDS flood warnings for these situations. For this reason, FDS users are cautioned to verify FDS estimates during the monsoon period and for regulated rivers before implementing flood management practices. Planned improvements by FDS developers involving physically-based hydrologic modeling should transform the system into a more accurate tool for near Hal-time decision making on flood management for ungauged river basins of the world. (c) 2010 Elsevier B.V. All rights reserved.
C1 [Moffitt, Caitlin Balthrop; Hossain, Faisal] Tennessee Technol Univ, Dept Civil & Environm Engn, Cookeville, TN 38505 USA.
[Adler, Robert F.; Yilmaz, Koray K.] Univ Maryland, College Pk, MD 20742 USA.
[Pierce, Harold F.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Pierce, Harold F.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Hossain, F (reprint author), Tennessee Technol Univ, Dept Civil & Environm Engn, 1020 Stadium Dr,Box 5015, Cookeville, TN 38505 USA.
EM fhossain@tntech.edu
RI Yilmaz, Koray/A-6053-2010
OI Yilmaz, Koray/0000-0002-6244-8826
FU NASA [NNX08AR32G]
FX The ground validation datasets used in this study were available through
an agreement between Institute of Water Modeling (Bangladesh) and
Tennessee Technological University. This study was supported by the NASA
New Investigator Program Award (NNX08AR32G) for author Faisal Hossain.
NR 28
TC 9
Z9 9
U1 1
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD APR
PY 2011
VL 13
IS 2
BP 165
EP 177
DI 10.1016/j.jag.2010.11.003
PG 13
WC Remote Sensing
SC Remote Sensing
GA 728SN
UT WOS:000287894900001
ER
PT J
AU He, LM
Chen, JM
Zhang, SL
Gomez, G
Pan, YD
McCullough, K
Birdsey, R
Masek, JG
AF He, Liming
Chen, Jing M.
Zhang, Shaoliang
Gomez, Gustavo
Pan, Yude
McCullough, Kevin
Birdsey, Richard
Masek, Jeffrey G.
TI Normalized algorithm for mapping and dating forest disturbances and
regrowth for the United States
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Article
DE Forest disturbance; The continental US; Fire; Logging; Disturbance
index; Change detection algorithm
ID FIRE SEVERITY; VEGETATION; INVENTORY; HISTORY; SINKS; WATER; AGE; US
AB Forest disturbances such as harvesting, wildfire and insect infestation are critical ecosystem processes affecting the carbon cycle. Because carbon dynamics are related to time since disturbance, forest stand age that can be used as a surrogate for major clear-cut/fire disturbance information has recently been recognized as an important input to forest carbon cycle models for improving prediction accuracy. In this study, forest disturbances in the USA for the period of similar to 1990-2000 were mapped using 400+ pairs of re-sampled Landsat TM/ETM scenes in 500m resolution, which were provided by the Landsat Ecosystem Disturbance Adaptive Processing System project. The detected disturbances were then separated into two five-year age groups, facilitated by Forest Inventory and Analysis (FIA) data, which was used to calculate the area of forest regeneration for each county in the USA.
In this study, a disturbance index (DI) was defined as the ratio of the short wave infrared (SWIR, band 5) to near-infrared (NIR, band 4) reflectance. Forest disturbances were identified through the Normalized Difference of Disturbance Index (NDDI) between circa 2000 and 1990, where a positive NDDI means disturbance and a negative NDDI means regrowth. Axis rotation was performed on the plot between DIs of the two matched Landsat scenes in order to reduce any difference of DIs caused by non-disturbance factors. The threshold of NDDI for each TM/ETM pair was determined by analysis of FIA data. Minor disturbances affecting small areas may be omitted due to the coarse resolution of the aggregated Landsat data, but the major stand-clearing disturbances (clear-cut harvest, fire) are captured. The spatial distribution of the detected disturbed areas was validated by Monitoring Trends in Burn Severity fire data in four States of the western USA (Washington, Oregon, Idaho, and California). Results indicate omission errors of 66.9%.
An important application of this remote sensing-based disturbance map is to associate with HA forest age data for developing a US forest age map. The US forest age map was also combined with the Canadian forest age map to produce a continent-wide forest map, which becomes a remarkable data layer for North America carbon cycle modeling. (c) 2010 Elsevier B.V. All rights reserved.
C1 [He, Liming; Chen, Jing M.] Univ Toronto, Dept Geog, Toronto, ON M5S 3G3, Canada.
[He, Liming; Chen, Jing M.] Univ Toronto, Program Planning, Toronto, ON M5S 3G3, Canada.
[Zhang, Shaoliang] China Univ Min & Technol, Xuzhou 221008, Jiangsu, Peoples R China.
[Gomez, Gustavo] Ryerson Univ, Toronto, ON M5B 2K3, Canada.
[Pan, Yude; McCullough, Kevin; Birdsey, Richard] US Forest Serv, USDA, Newtown Sq, PA 19073 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch Code 614 4, Greenbelt, MD 20771 USA.
RP He, LM (reprint author), Univ Toronto, Dept Geog, 100 St George St,Room 5047, Toronto, ON M5S 3G3, Canada.
EM liming.he@gmail.com; chenj@geog.utoronto.ca
RI Masek, Jeffrey/D-7673-2012; Pan, Yude/F-6145-2015;
OI He, Liming/0000-0003-4010-6814
FU US forest service
FX The authors are grateful to Dr. John Holm and Dr. Ziliang Zhu for their
support in this project. We thank Jeffrey G. Masek for providing the
Landsat TM/ETM data in 500 m resolution and LEDAPS product. We also
thank the US forest service for funding to conduct this research. The
authors thank the two anonymous reviewers for their valuable suggestions
on the manuscript.
NR 29
TC 13
Z9 14
U1 0
U2 32
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD APR
PY 2011
VL 13
IS 2
BP 236
EP 245
DI 10.1016/j.jag.2010.12.003
PG 10
WC Remote Sensing
SC Remote Sensing
GA 728SN
UT WOS:000287894900007
ER
PT J
AU Tripathi, N
Bell, LD
Nikzad, S
Tungare, M
Suvarna, PH
Sandvik, FS
AF Tripathi, Neeraj
Bell, L. D.
Nikzad, Shouleh
Tungare, Mihir
Suvarna, Puneet H.
Sandvik, Fatemeh Shahedipour
TI Novel Cs-Free GaN Photocathodes
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article; Proceedings Paper
CT 52nd Electronic Materials Conference (EMC)
CY JUN 23-25, 2010
CL Notre Dame, IN
DE GaN; photocathode; cesiated; detectors; MOCVD; photoemission
AB We report on a novel GaN photocathode structure that eliminates the use of Cs for photocathode activation. Development of such a photocathode structure promises reduced cost and complexity of the device, potentially with stable operation for a longer time. Device simulation studies suggest that deposition of Si delta-doped GaN on p-GaN templates induces sharp downward energy band bending at the surface, assisting in achieving effective negative electron affinity for GaN photocathodes without the use of Cs. A series of experiments has been performed to optimize the quality of the Si delta-doped layer to minimize the emission threshold of the device. This report includes significant observations relating the dependence of device properties such as emission threshold, quantum efficiency, and surface morphology on the Si incorporation in the Si delta-doped layer. An optimum Si incorporation has been observed to provide the minimum emission threshold of 4.1 eV for the discussed Cs-free GaN photocathodes. Photoemission (PE), atomic force microscopy (AFM), and secondary-ion mass spectroscopy (SIMS) have been performed to study the effect of growth conditions on device performance.
C1 [Tripathi, Neeraj; Tungare, Mihir; Suvarna, Puneet H.; Sandvik, Fatemeh Shahedipour] SUNY Albany, Coll Nanoscale Sci & Engn, Albany, NY 12203 USA.
[Bell, L. D.; Nikzad, Shouleh] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tripathi, N (reprint author), SUNY Albany, Coll Nanoscale Sci & Engn, Albany, NY 12203 USA.
EM sshahedipour@uamail.albany.edu
NR 15
TC 4
Z9 6
U1 2
U2 13
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD APR
PY 2011
VL 40
IS 4
BP 382
EP 387
DI 10.1007/s11664-010-1507-7
PG 6
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA 726XB
UT WOS:000287759100005
ER
PT J
AU Virshup, A
Liu, F
Lukco, D
Buchholt, K
Spetz, AL
Porter, LM
AF Virshup, Ariel
Liu, Fang
Lukco, Dorothy
Buchholt, Kristina
Spetz, Anita Lloyd
Porter, Lisa M.
TI Improved Thermal Stability Observed in Ni-Based Ohmic Contacts to n-Type
SiC for High-Temperature Applications
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article; Proceedings Paper
CT 52nd Electronic Materials Conference (EMC)
CY JUN 23-25, 2010
CL Notre Dame, IN
DE Ohmic contacts; silicon carbide; high-temperature reliability; scanning
electron microscopy; transmission electron microscopy
AB The high-temperature stability of a Pt/TaSi2/Ni/SiC ohmic contact metallization scheme was characterized using a combination of current-voltage measurements, Auger electron spectroscopy, and transmission electron microscopy imaging and associated analytical techniques. Increasing the thicknesses of the Pt and TaSi2 layers promoted electrical stability of the contacts, which remained ohmic at 600A degrees C in air for the extent of heat treatment; the specific contact resistance showed only a gradual increase from an initial value of 5.2 x 10(-5) Omega cm(2). We observed a continuous silicon oxide layer in the thinner contact structures, which failed after 36 h of heating. Meanwhile, thicker contacts with enhanced stability contained a much lower oxygen concentration that was distributed across the contact layers, precluding the formation of an electrically insulating contact structure.
C1 [Virshup, Ariel; Liu, Fang; Porter, Lisa M.] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
[Lukco, Dorothy] NASA, Glenn Res Ctr, ASRC Aerosp Corp, Cleveland, OH 44135 USA.
[Buchholt, Kristina; Spetz, Anita Lloyd] Linkoping Univ, S-58183 Linkoping, Sweden.
RP Virshup, A (reprint author), Carnegie Mellon Univ, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
EM avirshup@alumni.cmu.edu; fangl@andrew.cmu.edu; kribu@ifm.liu.se;
spetz@ifm.liu.se; lporter@andrew.cmu.edu
RI Lloyd Spetz, Anita/A-3834-2013
OI Lloyd Spetz, Anita/0000-0002-2817-3574
FU National Science Foundation [DMR-0304508, DMR-9802917]; Pennsylvania
Infrastructure Technology Alliance; Swedish Research Council; Swedish
Governmental Agency for Innovation Systems; Swedish Industry
FX The research at Carnegie Mellon was supported by the National Science
Foundation under Award No. DMR-0304508 and by the Pennsylvania
Infrastructure Technology Alliance. Metal films in this study were grown
using equipment funded by the National Science Foundation (Grant#
DMR-9802917). Additional Grants are acknowledged from the Swedish
Research Council, the Swedish Governmental Agency for Innovation Systems
and Swedish Industry.
NR 9
TC 7
Z9 7
U1 0
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD APR
PY 2011
VL 40
IS 4
BP 400
EP 405
DI 10.1007/s11664-010-1449-0
PG 6
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA 726XB
UT WOS:000287759100008
ER
PT J
AU DellaCorte, C
Bruckner, RJ
AF DellaCorte, Christopher
Bruckner, Robert J.
TI Remaining Technical Challenges and Future Plans for Oil-Free
Turbomachinery
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
ASME
LA English
DT Article
ID FOIL AIR BEARINGS; PERFORMANCE; DESIGN
AB The application of oil-free technologies (foil gas bearings, solid lubricants, and advanced analysis and predictive modeling tools) to advanced turbomachinery has been underway for several decades. During that time, full commercialization has occurred in aircraft air cycle machines, turbocompressors, cryocoolers, and ever-larger microturbines. Emerging products in the automotive sector (turbochargers and superchargers) indicate that a high volume serial production of foil bearings is imminent. The demonstration of foil bearings in auxiliary power units and select locations in propulsion gas turbines illustrates that such technology also has a place in these future systems. Foil bearing designs, predictive tools, and advanced solid lubricants that can satisfy anticipated requirements have been reported, but a major question remains regarding the scalability of foil bearings to ever-larger sizes to support heavier rotors. In this paper, the technological history, primary physics, engineering practicalities, and existing experimental and experiential database for scaling foil bearings are reviewed, and the major remaining technical challenges are identified.
C1 [DellaCorte, Christopher; Bruckner, Robert J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM christopher.dellacorte@nasa.gov; robert.j.bruckner@nasa.gov
NR 30
TC 11
Z9 12
U1 2
U2 9
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD APR
PY 2011
VL 133
IS 4
AR 042502
DI 10.1115/1.4002271
PG 7
WC Engineering, Mechanical
SC Engineering
GA 684IM
UT WOS:000284543600013
ER
PT J
AU Liu, YM
Larson, ME
Israelsson, UE
AF Liu, Yuanming
Larson, Melora E.
Israelsson, Ulf E.
TI Search for Enhancement of the Isobaric Thermal Expansion Coefficient of
Superfluid He-4 near T (lambda) by a Heat Current
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Thermal expansion coefficient; Superfluid helium; Heat current
ID FLOW INDUCED ANOMALIES; TRANSITION; PRESSURE; TEMPERATURE; CRITICALITY;
LIQUID-HE-4; GRAVITY; FLUX; HE4
AB We report an experimental search for the enhancement of the isobaric thermal expansion coefficient (beta (P) ) of superfluid He-4 near the superfluid transition by a heat current (Q). The experiment was carried out using the hot volume technique at constant sample pressure of 1 bar. Liquid helium was contained in a thermal conductivity cell, and a constant heat current, Q=10 or 100 mu W/cm(2), was supplied from below through the sample column. We performed a sample density calculation based on existing helium properties known in the literature and a proposed enhancement Delta beta (P) (Q). Both calculations, with or without the beta (P) enhancement, agree qualitatively with the measurement. The lack of definitive differentiation indicates that the beta (P) enhancement cannot be definitively resolved by our measurement in spite of applications of high-resolution thermometry and pressure regulation.
C1 [Liu, Yuanming; Larson, Melora E.; Israelsson, Ulf E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Liu, YM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Yuanming.Liu@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 22
TC 0
Z9 0
U1 0
U2 1
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2011
VL 163
IS 1-2
BP 13
EP 25
DI 10.1007/s10909-010-0273-5
PG 13
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 726WQ
UT WOS:000287757900002
ER
PT J
AU Bigelow, GS
Garg, A
Padula, SA
Gaydosh, DJ
Noebe, RD
AF Bigelow, G. S.
Garg, A.
Padula, S. A., II
Gaydosh, D. J.
Noebe, R. D.
TI Load-biased shape-memory and superelastic properties of a precipitation
strengthened high-temperature Ni50.3Ti29.7Hf20 alloy
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Shape memory alloys; Martensitic phase transformation; Precipitation;
Tension test; Transformation strain
ID TRANSFORMATION
AB A slightly Ni-rich NiTi-20Hf (at.%) alloy was aged for 3 h at 550 degrees C to form a homogeneous distribution of 10-20 nm precipitates. To determine the effect of such structures on the martensite-austenite transformation, preliminary load-biased shape-memory and superelastic properties were measured. The alloy exhibited reasonably high transformation temperatures, near-perfect dimensional stability and a work output as high as 18.7 J cm(-3) during load-biased thermal cycling. Isothermal stress cycling of the austenite between 180 and 220 degrees C resulted in near-perfect superelastic behavior up to 3% applied strain. Published by Elsevier Ltd. on behalf of Acta Materialia Inc.
C1 [Bigelow, G. S.; Garg, A.; Padula, S. A., II; Gaydosh, D. J.; Noebe, R. D.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44109 USA.
[Garg, A.] Univ Toledo, Toledo, OH 43606 USA.
[Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
RP Bigelow, GS (reprint author), NASA, Struct & Mat Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44109 USA.
EM glen.s.bigelow@nasa.gov; Anita.Garg-1@nasa.gov;
Darrell.J.Gaydosh@nasa.gov
FU NASA
FX This work was supported by the NASA Fundamental Aeronautics Program,
Supersonics Project.
NR 11
TC 57
Z9 59
U1 1
U2 16
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 APR
PY 2011
VL 64
IS 8
BP 725
EP 728
DI 10.1016/j.scriptamat.2010.12.028
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 728XR
UT WOS:000287908300009
ER
PT J
AU Kibanova, D
Trejo, M
Destaillats, H
Cervini-Silva, J
AF Kibanova, Daria
Trejo, Martin
Destaillats, Hugo
Cervini-Silva, Javiera
TI Photocatalytic activity of kaolinite
SO CATALYSIS COMMUNICATIONS
LA English
DT Article
DE Photocatalysis; Photolysis; Kaolinite; Degradation; Toluene; Methylene
blue
ID METHYLENE-BLUE; CLAY-MINERALS; ADSORPTION; PHOTODEGRADATION; SOIL;
POLLUTANTS; SURFACES; AIR; NANOCOMPOSITES; DECOMPOSITION
AB The photocatalytic activity of commercial kaolinite (KGa-1b) was evaluated for the degradation of methylene blue (MB) in aqueous suspension and of toluene in the gas phase. An enhanced photolysis of MB in the presence of kaolinite was detected, albeit at a slower rate than in the presence of the same mass of commercial TiO2 P25. Toluene removal under realistic ambient concentrations was catalyzed by both KGa-1b and P25; however, on a TiO2 content normalized basis, the clay mineral showed a higher photocatalytic rate. In the latter case, toluene degradation was found to be coupled to the presence of kaolinite surfaces, and not proportional to TiO2 content. (c) 2010 Elsevier B.V. All rights reserved.
C1 [Kibanova, Daria] Univ Nacl Autonoma Mexico, Fac Quim, Mexico City 04510, DF, Mexico.
[Kibanova, Daria; Cervini-Silva, Javiera] Univ Autonoma Metropolitana, Dept Proc & Tecnol, Unidad Cuajimalpa, Mexico City 01120, DF, Mexico.
[Trejo, Martin] Inst Politecn Nacl, ESIQIE, Mexico City 07738, DF, Mexico.
[Destaillats, Hugo] Lawrence Berkeley Natl Lab, Environm Energy Technol Div, Berkeley, CA USA.
[Destaillats, Hugo] Arizona State Univ, Dept Civil & Environm Engn, Tempe, AZ 85287 USA.
[Cervini-Silva, Javiera] Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA USA.
[Cervini-Silva, Javiera] NASA, Astrobiol Inst, Washington, DC 20546 USA.
RP Cervini-Silva, J (reprint author), Univ Autonoma Metropolitana, Dept Proc & Tecnol, Div Ciencias Nat & Ingn, Unidad Cuajimalpa UAM C, Artificios 40,40,6 Piso, Mexico City 01120, DF, Mexico.
EM jcervini@correo.cua.uam.mx
RI Destaillats, Hugo/B-7936-2013
FU Universidad Autonoma Metropolitana; CONACYT [23496]
FX The authors thank Maria del Rocio Galindo Ortega (Universidad Autonoma
Metropolitana Unidad Cuajimalpa) and Pilar Fernandez-Lomelin (Instituto
de Geografia, UNAM) for technical assistance. This project was supported
in part by Universidad Autonoma Metropolitana and ECACORE 2020 (SEMARNAT
CONACYT 23496).
NR 35
TC 6
Z9 6
U1 0
U2 25
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1566-7367
J9 CATAL COMMUN
JI Catal. Commun.
PD MAR 31
PY 2011
VL 12
IS 8
BP 698
EP 702
DI 10.1016/j.catcom.2010.10.029
PG 5
WC Chemistry, Physical
SC Chemistry
GA 741PM
UT WOS:000288875900003
ER
PT J
AU West, RA
Balloch, J
Dumont, P
Lavvas, P
Lorenz, R
Rannou, P
Ray, T
Turtle, EP
AF West, Robert A.
Balloch, Jonathan
Dumont, Philip
Lavvas, Panayotis
Lorenz, Ralph
Rannou, Pascal
Ray, Trina
Turtle, Elizabeth P.
TI The evolution of Titan's detached haze layer near equinox in 2009
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID UPPER-ATMOSPHERE; AEROSOLS; MESOSPHERE; ASYMMETRY; IMAGES; SATURN
AB Saturn's moon Titan has a massive atmosphere laden with layers of photochemical haze. We report a recent dramatic change in the vertical structure of this haze, with a persistent 'detached' layer dropping in altitude from over 500 km to only 380 km between 2007 and 2010. The detached haze layer appears to be a well-defined tracer for Titan's meridional stratospheric circulation, models of which suggest that a pole-to-pole meridional cell weakens during equinox as solar heating becomes more symmetric. These measurements connect the Cassini observations with those made by Voyager almost one seasonal cycle earlier. They place detailed constraints on the seasonal circulation, on the sources of photochemical aerosols, on the microphysical processes and on the complex interplay of these components. Citation: West, R. A., J. Balloch, P. Dumont, P. Lavvas, R. Lorenz, P. Rannou, T. Ray, and E. P. Turtle (2011), The evolution of Titan's detached haze layer near equinox in 2009, Geophys. Res. Lett., 38, L06204, doi: 10.1029/2011GL046843.
C1 [West, Robert A.; Balloch, Jonathan; Dumont, Philip; Ray, Trina] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lavvas, Panayotis] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Lorenz, Ralph; Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Rannou, Pascal] Univ Reims, GSMA, UMR 6089, CNRS, F-51687 Reims 2, France.
[Rannou, Pascal] Univ Versailles St Quentin, LATMOS, UMR 8190, CNRS, Verrieres Le Buisson, France.
RP West, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.a.west@jpl.nasa.gov
RI RANNOU, Pascal/I-9059-2012; Turtle, Elizabeth/K-8673-2012; Lorenz,
Ralph/B-8759-2016
OI Turtle, Elizabeth/0000-0003-1423-5751; Lorenz, Ralph/0000-0001-8528-4644
FU NASA; NASA Astrobiology Institute; Cassini Project
FX Part of this work was performed by the Jet Propulsion Laboratory,
California Institute of Technology, funded by the NASA Astrobiology
Institute and by the Cassini Project. RL was supported by the NASA
Cassini Data Analysis Program. We thank M. Evans for work on the optical
navigation of one image, and C. Porco who helped with an early version
of the paper.
NR 21
TC 25
Z9 25
U1 1
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 31
PY 2011
VL 38
AR L06204
DI 10.1029/2011GL046843
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 744IS
UT WOS:000289088700001
ER
PT J
AU Siegler, MA
Bills, BG
Paige, DA
AF Siegler, Matthew A.
Bills, Bruce G.
Paige, David A.
TI Effects of orbital evolution on lunar ice stability
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID SOUTH-POLE; COLD TRAPS; SPIN AXIS; WATER ICE; MOON; MERCURY; MARS;
DEPOSITS; SURFACE; OBLIQUITY
AB Many regions near the lunar poles are currently cold enough that surface water ice would be stable against sublimation losses for billions of years. However, most of these environments are currently too cold to efficiently drive ice downward by thermal diffusion, leaving impact burial as the primary means of protection from surface loss processes. In this respect, most of the present near-surface thermal environments on the Moon may actually be quite poor traps for water ice. This was not always the case. Long-term orbital changes have dramatically altered the lunar polar thermal environment. We develop a simple model of the evolution of the lunar orbit and spin axis to examine the thermal environments available for volatile deposition and retention in the past. Our calculations show that some early lunar polar environments were in the right temperature regime to have collected subsurface ice if a supply were available. However, a high-obliquity period, which occurred when the Moon was at about half its present distance from the Earth, would either have driven this ice out into space or deep into the lunar subsurface. Since that time, as the lunar obliquity has slowly decreased to its present value, environments have undergone their own thermal evolution, and each of the current cold traps experienced a period when they were most efficient at thermally burying ice. We examine the thermal history of a lunar polar crater to provide a framework for examining other processes effecting volatiles in the Moon's near-surface cold traps.
C1 [Siegler, Matthew A.; Paige, David A.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Bills, Bruce G.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Siegler, MA (reprint author), Univ Calif Los Angeles, 395 Charles Young Dr E, Los Angeles, CA 90095 USA.
EM siegler@ucla.edu; bills@jpl.nasa.gov; dap@mars.ucla.edu
NR 73
TC 27
Z9 28
U1 0
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 MAR 31
PY 2011
VL 116
AR E03010
DI 10.1029/2010JE003652
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 744HC
UT WOS:000289084500001
ER
PT J
AU McGregor, SL
Hughes, WJ
Arge, CN
Odstrcil, D
Schwadron, NA
AF McGregor, S. L.
Hughes, W. J.
Arge, C. N.
Odstrcil, D.
Schwadron, N. A.
TI The radial evolution of solar wind speeds
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MAGNETIC FIELDS; MAXIMUM; STREAM; MODEL
AB The WSA-ENLIL model predicts significant evolution of the solar wind speed. Along a flux tube the solar wind speed at 1.0 AU and beyond is found to be significantly altered from the solar wind speed in the outer corona at 0.1 AU, with most of the change occurring within a few tenths of an AU from the Sun. The evolution of the solar wind speed is most pronounced during solar minimum for solar wind with observed speeds at 1.0 AU between 400 and 500 km/s, while the fastest and slowest solar wind experiences little acceleration or deceleration. Solar wind ionic charge state observations made near 1.0 AU during solar minimum are found to be consistent with a large fraction of the intermediate-speed solar wind having been accelerated or decelerated from slower or faster speeds. This paper sets the groundwork for understanding the evolution of wind speed with distance, which is critical for interpreting the solar wind composition observations near Earth and throughout the inner heliosphere. We show from composition observations that the intermediate-speed solar wind (400-500 km/s) represents a mix of what was originally fast and slow solar wind, which implies a more bimodal solar wind in the corona than observed at 1.0 AU.
C1 [McGregor, S. L.; Hughes, W. J.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Arge, C. N.] Kirtland AFB, AFRL RVBXS, Space Vehicles Directorate, Albuquerque, NM 87117 USA.
[Odstrcil, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schwadron, N. A.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
RP McGregor, SL (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
EM slmic@bu.edu
FU National Science Foundation [ATM-0120950]
FX This work was supported by CISM, which is funded by the STC Program of
the National Science Foundation under cooperative agreement ATM-0120950.
I benefited from the availability of ACE SWICS (PI: T. Zurbuchan) and
SWEPAM (PI: D. McComas) data. We thank the National Solar Observatory
for providing access to their synoptic magnetogram data sets.
NR 23
TC 5
Z9 6
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR 31
PY 2011
VL 116
AR A03106
DI 10.1029/2010JA016006
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 744HB
UT WOS:000289084400003
ER
PT J
AU Bedding, TR
Mosser, B
Huber, D
Montalban, J
Beck, P
Christensen-Dalsgaard, J
Elsworth, YP
Garcia, RA
Miglio, A
Stello, D
White, TR
De Ridder, J
Hekker, S
Aerts, C
Barban, C
Belkacem, K
Broomhall, AM
Brown, TM
Buzasi, DL
Carrier, F
Chaplin, WJ
Di Mauro, MP
Dupret, MA
Frandsen, S
Gilliland, RL
Goupil, MJ
Jenkins, JM
Kallinger, T
Kawaler, S
Kjeldsen, H
Mathur, S
Noels, A
Aguirre, VS
Ventura, P
AF Bedding, Timothy R.
Mosser, Benoit
Huber, Daniel
Montalban, Josefina
Beck, Paul
Christensen-Dalsgaard, Jorgen
Elsworth, Yvonne P.
Garcia, Rafael A.
Miglio, Andrea
Stello, Dennis
White, Timothy R.
De Ridder, Joris
Hekker, Saskia
Aerts, Conny
Barban, Caroline
Belkacem, Kevin
Broomhall, Anne-Marie
Brown, Timothy M.
Buzasi, Derek L.
Carrier, Fabien
Chaplin, William J.
Di Mauro, Maria Pia
Dupret, Marc-Antoine
Frandsen, Soren
Gilliland, Ronald L.
Goupil, Marie-Jo
Jenkins, Jon M.
Kallinger, Thomas
Kawaler, Steven
Kjeldsen, Hans
Mathur, Savita
Noels, Arlette
Aguirre, Victor Silva
Ventura, Paolo
TI Gravity modes as a way to distinguish between hydrogen- and
helium-burning red giant stars
SO NATURE
LA English
DT Article
ID SOLAR-LIKE OSCILLATIONS; STELLAR OSCILLATIONS; COROT; ASTEROSEISMOLOGY;
KEPLER; CODE; MASS
AB Red giants are evolved stars that have exhausted the supply of hydrogenin their cores and instead burn hydrogen in a surrounding shell(1,2). Once a red giant is sufficiently evolved, the helium in the core also undergoes fusion(3). Outstanding issues in our understanding of red giants include uncertainties in the amount of mass lost at the surface before helium ignition and the amount of internal mixing from rotation and other processes(4). Progress is hampered by our inability to distinguish between red giants burning helium in the core and those still only burning hydrogen in a shell. Asteroseismology offers a way forward, being a powerful tool for probing the internal structures of stars using their natural oscillation frequencies(5). Here we report observations of gravity-mode period spacings in red giants(6) that permit a distinction between evolutionary stages to be made. We use high-precision photometry obtained by the Kepler spacecraft over more than a year to measure oscillations in several hundred red giants. We find many stars whose dipole modes show sequences with approximately regular period spacings. These stars fall into two clear groups, allowing us to distinguish unambiguously between hydrogen-shell-burning stars (period spacing mostly similar to 50 seconds) and those that are also burning helium (period spacing similar to 100 to 300 seconds).
C1 [Bedding, Timothy R.; Huber, Daniel; Stello, Dennis; White, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Mosser, Benoit; Barban, Caroline; Goupil, Marie-Jo] Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Montalban, Josefina; Miglio, Andrea; Dupret, Marc-Antoine; Noels, Arlette] Univ Liege, Inst Astrophys & Geophys, B-4000 Cointe Ougree, Belgium.
[Beck, Paul; De Ridder, Joris; Aerts, Conny; Carrier, Fabien] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Christensen-Dalsgaard, Jorgen; Frandsen, Soren] Aarhus Univ, Dept Phys & Astron, DASC, DK-8000 Aarhus C, Denmark.
[Elsworth, Yvonne P.; Miglio, Andrea; Hekker, Saskia; Broomhall, Anne-Marie; Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Garcia, Rafael A.] Univ Paris 07, Ctr Saclay, IRFU SAp, Lab AIM,CEA DSM CNRS, F-91191 Gif Sur Yvette, France.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Aerts, Conny] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Belkacem, Kevin] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Buzasi, Derek L.] Eureka Sci, Oakland, CA 94602 USA.
[Di Mauro, Maria Pia] Ist Astrofis Spaziale & Fis Cosm, INAF IASF, I-00133 Rome, Italy.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Kallinger, Thomas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Kawaler, Steven] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Mathur, Savita] NCAR, High Altitude Observ, Boulder, CO 80307 USA.
[Aguirre, Victor Silva] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Ventura, Paolo] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy.
RP Bedding, TR (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
EM t.bedding@physics.usyd.edu.au
OI Ventura, Paolo/0000-0002-5026-6400; Kallinger,
Thomas/0000-0003-3627-2561; Di Mauro, Maria Pia/0000-0001-7801-7484;
Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661;
Garcia, Rafael/0000-0002-8854-3776; Kawaler, Steven/0000-0002-6536-6367
FU NASA's Science Mission Directorate; Australian Research Council;
European Community; Netherlands Organisation for Scientific Research
(NWO); National Science Foundation
FX We acknowledge the entire Kepler team, whose efforts made these results
possible. We thank M. Biercuk for comments. Funding for this Discovery
mission was provided by NASA's Science Mission Directorate. T.R.B and
D.S. were supported by the Australian Research Council; P.B. and C.A.
were supported by European Community's 7th Framework Programme
(PROSPERITY); S.H. was supported by the Netherlands Organisation for
Scientific Research (NWO). The National Center for Atmospheric Research
is sponsored by the National Science Foundation.
NR 30
TC 209
Z9 209
U1 6
U2 28
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 MAR 31
PY 2011
VL 471
IS 7340
BP 608
EP 611
DI 10.1038/nature09935
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 742NN
UT WOS:000288951200036
PM 21455175
ER
PT J
AU Balaban, PM
Malyshev, AY
Ierusalimsky, VN
Aseyev, N
Korshunova, TA
Bravarenko, NI
Lemak, MS
Roshchin, M
Zakharov, IS
Popova, Y
Boyle, R
AF Balaban, Pavel M.
Malyshev, Aleksey Y.
Ierusalimsky, Victor N.
Aseyev, Nikolay
Korshunova, Tania A.
Bravarenko, Natasha I.
Lemak, M. S.
Roshchin, Matvey
Zakharov, Igor S.
Popova, Yekaterina
Boyle, Richard
TI Functional Changes in the Snail Statocyst System Elicited by
Microgravity
SO PLOS ONE
LA English
DT Article
ID STATIC VESTIBULOOCULAR REFLEX; HAIR-CELL; XENOPUS-LAEVIS; A
PHOTORECEPTORS; TERRESTRIAL SNAIL; LYMNAEA-STAGNALIS; HERMISSENDA;
NEURONS; HYPERGRAVITY; EXPRESSION
AB Background: The mollusk statocyst is a mechanosensing organ detecting the animal's orientation with respect to gravity. This system has clear similarities to its vertebrate counterparts: a weight-lending mass, an epithelial layer containing small supporting cells and the large sensory hair cells, and an output eliciting compensatory body reflexes to perturbations.
Methodology/Principal Findings: In terrestrial gastropod snail we studied the impact of 16-(Foton M-2) and 12-day (Foton M-3) exposure to microgravity in unmanned orbital missions on: (i) the whole animal behavior (Helix lucorum L.), (ii) the statoreceptor responses to tilt in an isolated neural preparation (Helix lucorum L.), and (iii) the differential expression of the Helix pedal peptide (HPep) and the tetrapeptide FMRFamide genes in neural structures (Helix aspersa L.). Experiments were performed 13-42 hours after return to Earth. Latency of body re-orientation to sudden 90 degrees head-down pitch was significantly reduced in postflight snails indicating an enhanced negative gravitaxis response. Statoreceptor responses to tilt in postflight snails were independent of motion direction, in contrast to a directional preference observed in control animals. Positive relation between tilt velocity and firing rate was observed in both control and postflight snails, but the response magnitude was significantly larger in postflight snails indicating an enhanced sensitivity to acceleration. A significant increase in mRNA expression of the gene encoding HPep, a peptide linked to ciliary beating, in statoreceptors was observed in postflight snails; no differential expression of the gene encoding FMRFamide, a possible neurotransmission modulator, was observed.
Conclusions/Significance: Upregulation of statocyst function in snails following microgravity exposure parallels that observed in vertebrates suggesting fundamental principles underlie gravi-sensing and the organism's ability to adapt to gravity changes. This simple animal model offers the possibility to describe general subcellular mechanisms of nervous system's response to conditions on Earth and in space.
C1 [Balaban, Pavel M.; Malyshev, Aleksey Y.; Ierusalimsky, Victor N.; Aseyev, Nikolay; Korshunova, Tania A.; Bravarenko, Natasha I.; Lemak, M. S.; Roshchin, Matvey] Russian Acad Sci, Inst Higher Nervous Act & Neurophysiol, Moscow, Russia.
[Zakharov, Igor S.] Russian Acad Sci, Koltzov Inst Dev Biol, Moscow, Russia.
[Popova, Yekaterina; Boyle, Richard] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Balaban, PM (reprint author), Russian Acad Sci, Inst Higher Nervous Act & Neurophysiol, Moscow, Russia.
EM balaban@ihna.msk.ru; richard.boyle@nasa.gov
RI Zakharov, Igor/K-5488-2013; Balaban, Pavel/I-5811-2014; Malyshev,
Alexey/P-2775-2015;
OI Balaban, Pavel/0000-0001-9248-8207; Malyshev,
Aleksey/0000-0002-4633-7691
FU RF President Council; Russian Foundation for Basic Research; Russian
Academy of Science; NASA [03-OBPR-04]; Fundamental Space Biology Program
FX This research was supported by grants from the RF President Council for
grants to P. Balaban, Russian Foundation for Basic Research, Russian
Academy of Science, NASA 03-OBPR-04 and a Fundamental Space Biology
Program grant to R. Boyle. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 75
TC 2
Z9 4
U1 1
U2 11
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 MAR 29
PY 2011
VL 6
IS 3
AR e17710
DI 10.1371/journal.pone.0017710
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 743YC
UT WOS:000289054600015
PM 21479267
ER
PT J
AU Huang, HG
Liu, QH
Qin, WH
Du, YM
Li, XW
AF Huang, Huaguo
Liu, Qinhuo
Qin, Wenhan
Du, Yongming
Li, Xiaowen
TI Temporal patterns of thermal emission directionality of crop canopies
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RADIATIVE SURFACE-TEMPERATURE; DUAL ANGLE OBSERVATIONS; HEAT-FLUX;
RADIOMETRIC TEMPERATURES; BRIGHTNESS TEMPERATURE; COMPONENT
TEMPERATURES; INFRARED RADIATION; ANGULAR VARIATIONS; DECIDUOUS FOREST;
NATURAL SURFACES
AB Many field experiments have observed significant temporal variations of thermal infrared (TIR) emission directionality, making it necessary to explain this phenomenon quantitatively to exploit potential applications of the directional remotely sensed TIR observation. The main objective of this paper is to determine when and how the significant directional effect appears. Two models, TRGM and Cupid, are linked to simulate the temporal variations of directional brightness temperature T-B(theta) of crop canopies, including winter wheat and summer corn. Two indicators are defined: (1) Delta T-B,T-AVG representing the mean difference between nadir T-B(0) and off-nadir T-B(55) and (2) Delta T-B,T-STD representing the standard deviation of T-B(55) for different view azimuth angles. Simulation results show that the highest DTB,AVG of up to 4 degrees C appears mostly at midday (1200-1300 LT), while the lowest Delta T-B,T- AVG appears mostly in the early morning (0700-0800 LT) or late afternoon (1700-1800 LT). The Delta(TB,STD) is about one third of Delta(TB,AVG) and should not be neglected given its considerable value at around 1400 LT. This trend has been proven through field measurements at both wheat and corn sites. The major factors affecting the trend are also identified using sensitivity analysis. Among the major factors, soil water content, LAI, and solar radiation are the three most significant factors, whereas the wind speed and air temperature have a larger effect on Delta(TB,AVG) than air humidity. It is interesting that Delta(TB,AVG) reaches a maximum value when the LAI is around 0.8. Further analysis shows that Delta(TB,AVG) is related to soil surface net radiation, which will be useful in net radiation estimation.
C1 [Huang, Huaguo] Beijing Forestry Univ, Minist Educ, Key Lab Silviculture & Conservat, Beijing 100083, Peoples R China.
[Huang, Huaguo; Liu, Qinhuo; Qin, Wenhan; Du, Yongming; Li, Xiaowen] Beijing Normal Univ, Chinese Acad Sci, Inst Remote Sensing Applicat, State Key Lab Remote Sensing Sci, Beijing 100101, Peoples R China.
[Qin, Wenhan] NASA, Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA.
RP Huang, HG (reprint author), Beijing Forestry Univ, Minist Educ, Key Lab Silviculture & Conservat, Beijing 100083, Peoples R China.
EM huaguo.huang@gmail.com
FU Chinese Natural Science Foundation [40801135, 40730525]; China's Special
Funds for Major State Basic Research Project [2007CB714402]; Fundamental
Research Funds for the Central Universities
FX This work was supported by the Chinese Natural Science Foundation
Project (40801135 and 40730525), China's Special Funds for Major State
Basic Research Project (2007CB714402), and the Fundamental Research
Funds for the Central Universities. We wish to thank the authors of the
4SAIL and DART models for providing us with the programs for comparison
and the reviewers for providing useful comments.
NR 68
TC 2
Z9 3
U1 7
U2 31
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 MAR 29
PY 2011
VL 116
AR D06114
DI 10.1029/2010JD014613
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 744HN
UT WOS:000289085600002
ER
PT J
AU Osipov, VV
Muratov, CB
Ponizovskaya-Devine, E
Foygel, M
Smelyanskiy, VN
AF Osipov, V. V.
Muratov, C. B.
Ponizovskaya-Devine, E.
Foygel, M.
Smelyanskiy, V. N.
TI Cavitation-induced ignition of cryogenic hydrogen-oxygen fluids
SO APPLIED PHYSICS LETTERS
LA English
DT Article
AB The Challenger disaster and purposeful experiments with liquid hydrogen (H2) and oxygen (Ox) tank breaches demonstrated that cryogenic H2/Ox fluids always self-ignite in the process of their sudden mixing. Here, we propose a cavitation-induced self-ignition mechanism that may be realized under these conditions. In one possible scenario, self-ignition is caused by the strong shock waves generated by the collapse of pure Ox vapor bubble near the surface of the Ox liquid that may initiate detonation of the gaseous H2/Ox mixture next to the gas-liquid interface. This effect is further enhanced by H2/Ox combustion inside the collapsing bubble in the presence of admixed H2 gas. (c) 2011 American Institute of Physics. [doi: 10.1063/1.3571445]
C1 [Osipov, V. V.; Ponizovskaya-Devine, E.; Foygel, M.; Smelyanskiy, V. N.] NASA, Ames Res Ctr, D&SH Branch, Intelligent Syst Div, Moffett Field, CA 94035 USA.
[Muratov, C. B.] New Jersey Inst Technol, Dept Math Sci, Newark, NJ 07102 USA.
RP Osipov, VV (reprint author), NASA, Ames Res Ctr, D&SH Branch, Intelligent Syst Div, MS 269-1, Moffett Field, CA 94035 USA.
EM viatcheslav.v.osipov@nasa.gov
FU NASA [NNX10AC65G]
FX The work of CBM was supported by NASA via Grant No. NNX10AC65G.
NR 10
TC 4
Z9 4
U1 1
U2 9
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 28
PY 2011
VL 98
IS 13
AR 134102
DI 10.1063/1.3571445
PG 3
WC Physics, Applied
SC Physics
GA 745GJ
UT WOS:000289153600104
ER
PT J
AU Sawicki, JT
Friswell, MI
Kulesza, Z
Wroblewski, A
Lekki, JD
AF Sawicki, Jerzy T.
Friswell, Michael I.
Kulesza, Zbigniew
Wroblewski, Adam
Lekki, John D.
TI Detecting cracked rotors using auxiliary harmonic excitation
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID TRANSVERSE CRACK; VIBRATION ANALYSIS; ROTATING SHAFT; BEARING;
IDENTIFICATION
AB Cracked rotors are not only important from a practical and economic viewpoint, they also exhibit interesting dynamics. This paper investigates the modelling and analysis of machines with breathing cracks, which open and close due to the self-weight of the rotor, producing a parametric excitation. After reviewing the modelling of cracked rotors, the paper analyses the use of auxiliary excitation of the shaft, often implemented using active magnetic bearings to detect cracks. Applying a sinusoidal excitation generates response frequencies that are combinations of the rotor spin speed and excitation frequency. Previously this system was analysed using multiple scales analysis; this paper suggests an alternative approach based on the harmonic balance method, and validates this approach using simulated and experimental results. Consideration is also given to some issues to enable this approach to become a robust condition monitoring technique for cracked shafts. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Sawicki, Jerzy T.] Cleveland State Univ, Ctr Rotating Machinery Dynam & Control RoMaDyC, Cleveland, OH 44115 USA.
[Friswell, Michael I.] Swansea Univ, Sch Engn, Swansea SA2 8PP, W Glam, Wales.
[Kulesza, Zbigniew] Bialystok Tech Univ, Fac Mech Engn, Bialystok, Poland.
[Wroblewski, Adam] ASRC Aerosp Inc, NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Wroblewski, Adam] NASA, ASRC Aerosp Inc, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Sawicki, JT (reprint author), Cleveland State Univ, Ctr Rotating Machinery Dynam & Control RoMaDyC, Cleveland, OH 44115 USA.
EM j.sawicki@csuohio.edu
RI Friswell, Michael/B-5581-2009; Kulesza, Zbigniew/M-5019-2013
OI Friswell, Michael/0000-0003-4677-7395; Kulesza,
Zbigniew/0000-0002-9521-0056
FU NASA [NNX08AC31A]
FX This research has been funded by NASA's Research Opportunities in
Aeronautics. Grant no. NNX08AC31A.
NR 29
TC 37
Z9 37
U1 0
U2 21
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 MAR 28
PY 2011
VL 330
IS 7
BP 1365
EP 1381
DI 10.1016/j.jsv.2010.10.006
PG 17
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA 724AW
UT WOS:000287549500006
ER
PT J
AU Andrew, A
Buffinger, DR
Street, KW
Scheiman, DA
AF Andrew, Alece
Buffinger, Delbert R.
Street, Kenneth W.
Scheiman, Daniel A.
TI Evolved gas profiles of lunar regolith simulants and their constituents
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Wilberforce Univ, Dept Nat Sci, Wilberforce, OH USA.
NASA, John Glenn Res Ctr, ASRC Aerosp Corp, Cleveland, OH USA.
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 MAR 27
PY 2011
VL 241
MA 657-CHED
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982800629
ER
PT J
AU Chambliss, RN
Srivastava, D
Makeev, M
Reeves, MS
AF Chambliss, Rozlyn N.
Srivastava, Deepak
Makeev, Maxim
Reeves, Melissa S.
TI Tensile and compressive deformation of polyethylene with varying
temperature and strain rates
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Tuskegee Univ, Ctr Adv Mat, Tuskegee, AL 36088 USA.
NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
NR 0
TC 0
Z9 0
U1 1
U2 5
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 MAR 27
PY 2011
VL 241
MA 42-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982805501
ER
PT J
AU Dinh, HN
Pylypenko, S
Dameron, A
Neyerlin, KC
Olson, T
Christensen, S
O'Neil, K
Hurst, KE
Bult, J
Corpuz, A
Narayan, SR
Karthik, A
Yang, B
Hays, CC
Johnson, MA
O'Hayre, R
Pivovar, B
Gennett, T
AF Dinh, Huyen N.
Pylypenko, Svitlana
Dameron, Arrelaine
Neyerlin, K. C.
Olson, Timothy
Christensen, Steven
O'Neil, Kevin
Hurst, Katherine E.
Bult, Justin
Corpuz, April
Narayan, S. R.
Karthik, Ashwin
Yang, Bo
Hays, Charles C.
Johnson, M. A.
O'Hayre, Ryan
Pivovar, Bryan
Gennett, Thomas
TI Enhancing the methanol oxidation catalyst activity and durability via
affecting the catalyst-support interaction
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Natl Renewable Energy Lab, Golden, CO USA.
Colorado Sch Mines, Dept Met & Mat Engn, Golden, CO 80401 USA.
Univ So Calif, Dept Chem, Los Angeles, CA 90089 USA.
CALTECH, Jet Prop Lab, Pasadena, CA USA.
RI O'Hayre, Ryan/A-8183-2009
NR 0
TC 0
Z9 0
U1 2
U2 9
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 MAR 27
PY 2011
VL 241
MA 317-FUEL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982804742
ER
PT J
AU Forsley, LP
Mosier-Boss, P
Tanzella, F
Lipson, A
Zhou, DZ
Roussetski, A
McKubre, M
AF Forsley, Lawrence P.
Mosier-Boss, Pamela
Tanzella, Francis
Lipson, Andrei
Zhou, Dazhuang
Roussetski, Alexi
McKubre, Michael
TI Comparison of three methods of analyzing nuclear tracks observed in
CR-39 detectors used in Pd/D co-deposition experiments
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 JWK Int Corp, Dept Emerging Technol, Annandale, VA USA.
SPAWAR Syst Ctr Pacific, San Diego, CA USA.
SRI, Menlo Pk, CA USA.
Russian Acad Sci, Inst Phys Chem, Moscow, Russia.
NASA, Johnson Space Flight Ctr, Univ Space Res Assoc, Houston, TX USA.
Russian Acad Sci, PN Lebedev Phys Inst, Moscow, Russia.
NR 0
TC 0
Z9 0
U1 0
U2 3
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 MAR 27
PY 2011
VL 241
MA 33-ENVR
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982804373
ER
PT J
AU Frank, JV
Amashukeli, X
Fisher, A
AF Frank, Jill V.
Amashukeli, Xenia
Fisher, Anita
TI RF-powered micro-extractor sample injection protocol development
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Union Univ, Dept Chem, Jackson, TN 38305 USA.
CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
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 MAR 27
PY 2011
VL 241
MA 206-CHED
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982800230
ER
PT J
AU Guo, HQ
Meador, MAB
Sprowl, G
AF Guo, Haiquan
Meador, Mary Ann B.
Sprowl, Guilherme
TI Polyimide aerogels with amine functionalized polysilsesquioxane
cross-links
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Ohio Aerosp Inst, Cleveland, OH USA.
NASA, Glenn Res Ctr, Cleveland, OH USA.
Rose Hulman Inst Technol, Terre Haute, IN 47803 USA.
NR 0
TC 0
Z9 0
U1 1
U2 7
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 MAR 27
PY 2011
VL 241
MA 327-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982802879
ER
PT J
AU Hurwitz, FI
Guo, HQ
Newlin, KN
AF Hurwitz, Frances I.
Guo, Haiquan
Newlin, Katy N.
TI Influence of Boehmite precursor on aluminosilicate aerogel pore
structure, phase stability and resistance to densification at high
temperatures
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH USA.
Ohio Aerosp Inst, Cleveland, OH USA.
Univ Louisville, Louisville, KY USA.
NR 0
TC 0
Z9 0
U1 1
U2 4
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 MAR 27
PY 2011
VL 241
MA 316-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982807359
ER
PT J
AU Jack, CC
Duffy, NV
Hepp, AF
Hoops, MD
AF Jack, Colin C.
Duffy, Norman V.
Hepp, Aloysius F.
Hoops, Michael D.
TI Studying the thermal decompostion pathways of iron dithiocarbamates
using a thermogravimetric analyzer
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Wheeling Jesuit Univ, Dept Chem, Wheeling, WV USA.
NASA, Space Proc & Expt Div, Glenn Res Ctr, Cleveland, OH USA.
NR 0
TC 0
Z9 0
U1 0
U2 3
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 MAR 27
PY 2011
VL 241
MA 686-CHED
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982800656
ER
PT J
AU Kokkila, SIL
Bera, PP
Francisco, JS
Lee, TJ
AF Kokkila, Sara I. L.
Bera, Partha P.
Francisco, Joseph S.
Lee, Timothy J.
TI Group increment scheme for IR absorption intensities of greenhouse gases
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Coll St Benedict, Dept Chem, St Joseph, MN USA.
Coll St Benedict, Dept Math, St Joseph, MN USA.
St Johns Univ, St Joseph, MN USA.
Ames Res Ctr, Div Space Sci & Astrobiol, Natl Aeronaut & Space Adm, Mountain View, CA USA.
Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
NR 0
TC 0
Z9 0
U1 0
U2 3
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 MAR 27
PY 2011
VL 241
MA 1118-CHED
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982801084
ER
PT J
AU Krause, FC
Smart, MC
Bugga, RV
Prakash, GKS
AF Krause, Frederick C.
Smart, Marshall C.
Bugga, Ratnakumar V.
Prakash, G. K. Surya
TI Fluorinated electrolytes in lithium-ion batteries for improved safety in
manned-flight and terrestrial applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Univ So Calif, Dept Chem, Loker Hydrocarbon Res Inst, Los Angeles, CA 90089 USA.
CALTECH, Jet Prop Lab, Pasadena, CA USA.
NR 0
TC 0
Z9 0
U1 3
U2 7
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 MAR 27
PY 2011
VL 241
MA 177-FUEL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982804695
ER
PT J
AU Lenz, OM
Meyyappan, M
Nguyen, CV
AF Lenz, Olivia M.
Meyyappan, M.
Nguyen, Cattien V.
TI Chemical synthesis of lead zirconate titanate nanowires
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Seattle Pacific Univ, Dept Chem & Biochem, Seattle, WA 98119 USA.
NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
ELORET Corp, Moffett Field, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 3
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 MAR 27
PY 2011
VL 241
MA 789-CHED
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982800757
ER
PT J
AU Meador, MAB
Malow, EJ
He, ZHJ
McCorkle, L
AF Meador, Mary Ann B.
Malow, Ericka J.
He, Zuohui J.
McCorkle, Linda
TI Improvements to synthesis of polyimide aerogels
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 NASA, Glenn Res Ctr, Cleveland, OH USA.
Ohio Aerosp Inst, Cleveland, OH USA.
NR 0
TC 0
Z9 1
U1 1
U2 9
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 MAR 27
PY 2011
VL 241
MA 262-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982807356
ER
PT J
AU Sakamoto, JS
Maloney, RP
Thompson, T
Schock, H
Jones, SM
Paik, J
AF Sakamoto, Jeff S.
Maloney, Ryan P.
Thompson, Travis
Schock, Harold
Jones, Steven M.
Paik, Jay
TI High temperature aerogel insulation for space and terrestrial
thermal-to-electric energy conversion
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 MSU, CHEMS, E Lansinsg, ME USA.
CALTECH, Jet Prop Lab, Pasadena, CA USA.
RI Maloney, Ryan/G-3834-2012
OI Maloney, Ryan/0000-0002-6158-1537
NR 0
TC 0
Z9 0
U1 1
U2 4
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 MAR 27
PY 2011
VL 241
MA 315-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982807358
ER
PT J
AU Vilozny, B
Actis, P
Seger, RA
Pourmand, N
AF Vilozny, Boaz
Actis, Paolo
Seger, Ronald A.
Pourmand, Nader
TI Selective and transient current blockage by precipitation in conical
quartz nanopores
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 241st National Meeting and Exposition of the American-Chemical-Society
(ACS)
CY MAR 27-31, 2011
CL Anaheim, CA
SP Amer Chem Soc
C1 Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA.
NASA, Adv Studies Labs, Bioinfonano Res & Dev Inst, Ames Res Ctr, Moffett Field, CA USA.
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 MAR 27
PY 2011
VL 241
MA 1135-INOR
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 782BO
UT WOS:000291982805181
ER
PT J
AU Velazco, VA
Toon, GC
Blavier, JFL
Kleinbohl, A
Manney, GL
Daffer, WH
Bernath, PF
Walker, KA
Boone, C
AF Velazco, Voltaire A.
Toon, Geoffrey C.
Blavier, Jean-Francois L.
Kleinboehl, Armin
Manney, Gloria L.
Daffer, William H.
Bernath, Peter F.
Walker, Kaley A.
Boone, Chris
TI Validation of the Atmospheric Chemistry Experiment by noncoincident MkIV
balloon profiles
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID FOURIER-TRANSFORM SPECTROMETER; ACE-FTS; LOWER STRATOSPHERE; UPPER
TROPOSPHERE; SATELLITE; INSTRUMENT; METHANE; CLONO2; SPACE; WATER
AB We have compared volume mixing ratio profiles of atmospheric trace gases measured by the Atmospheric Chemistry Experiment (ACE) version 2.2 and the MkIV solar occultation Fourier transform infrared spectrometers. These gases are H2O, O-3, N2O, CO, CH4, HNO3, HF, HCl, OCS, ClONO2, HCN, CH3Cl, CF4, CCl2F2, CCl3F, COF2, CHF2Cl, and SF6. Due to the complete lack of close spatiotemporal coincidences between the ACE occultations and the MkIV balloon flights, we used potential temperatures and equivalent latitudes from analyzed meteorological fields to find comparable ACE and MkIV profiles. The results show excellent agreement for CH4, N2O, and other long-lived gases but slightly poorer agreement for shorter-lived species like CO, O-3, and HCN. For example, in the upper troposphere (similar to 400-650 K), maximum differences between MkIV and ACE are 2.4% for CH4, 1.7% for N2O, -12.4% for CO, -15.9% for O-3, and -5.6% for HCN. In the lower stratosphere (similar to 650-900 K), maximum MkIV-ACE differences are 7.6% for CH4, 14.1% for N2O, 7.3% for CO, -9.2% for O-3, and 31.5% for HCN. Apart from a small vertical misregistration problem, the overall agreement between MkIV and ACE is very good.
C1 [Velazco, Voltaire A.; Toon, Geoffrey C.; Blavier, Jean-Francois L.; Kleinboehl, Armin; Manney, Gloria L.; Daffer, William H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bernath, Peter F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England.
[Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Boone, Chris] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
RP Velazco, VA (reprint author), Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany.
EM voltaire@iup.physik.uni-bremen.de
RI Velazco, Voltaire/H-2280-2011; Bernath, Peter/B-6567-2012
OI Velazco, Voltaire/0000-0002-1376-438X; Bernath,
Peter/0000-0002-1255-396X
FU NASA; Canadian Space Agency; UK Natural Environment Research Council
(NERC)
FX We sincerely thank the three anonymous reviewers for their very
constructive comments and suggestions to improve the manuscript. We
thank the Columbia Scientific Ballooning Facility (CSBF), which
performed the balloon launches of the MkIV instrument described in this
work. Part of this research was conducted at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. The ACE mission is supported primarily by the Canadian Space
Agency. Some support was also provided by the UK Natural Environment
Research Council (NERC).
NR 38
TC 11
Z9 11
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 25
PY 2011
VL 116
AR D06306
DI 10.1029/2010JD014928
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 741LV
UT WOS:000288866100001
ER
PT J
AU Garcia, CAE
Garcia, VMT
Dogliotti, AI
Ferreira, A
Romero, SI
Mannino, A
Souza, MS
Mata, MM
AF Eiras Garcia, Carlos Alberto
Tavano Garcia, Virginia Maria
Dogliotti, Ana Ines
Ferreira, Amabile
Romero, Silvia I.
Mannino, Antonio
Souza, Marcio S.
Mata, Mauricio M.
TI Environmental conditions and bio-optical signature of a coccolithophorid
bloom in the Patagonian shelf
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID EASTERN ENGLISH-CHANNEL; CENTRAL NORTH-ATLANTIC; CHLOROPHYLL-A; OPTICAL
BACKSCATTERING; LIGHT-SCATTERING; EMILIANIA-HUXLEYI; ORGANIC-CARBON;
OCEAN COLOR; SOUTHWESTERN ATLANTIC; PARTICLE COMPOSITION
AB In January 2008, a patch of high reflectance detected by ocean color satellite images was sampled during a cruise over the southern Argentinean continental shelf. High calcite concentrations (particulate inorganic carbon (PIC)) found at the patch were associated with dominance of the coccolithophorid Emiliania huxleyi. Relatively low chlorophyll concentrations (0.29 to 1.48 mg m(-3)) were found, but both particulate attenuation (0.27 to 1.15 m(-1)) and backscattering coefficients at 660 nm (0.003 to 0.042 m(-1)) were noticeably high. Particulate inorganic to organic carbon (POC) ratio (PIC: POC) was highly variable (0.02 to 1.1), but mostly high, showing a significant correlation with particulate backscattering coefficient at 660 nm (r = 0.83, p < 0.005). The spectral dependency of the backscattering coefficient followed Gordon et al. (2009). Both the time evolution analyses of normalized water leaving radiance at 551 nm (nLw551) and the high PIC: POC ratios suggested an advanced stage of the coccolithophorid bloom, therefore with high detached coccoliths:cell ratios. Moreover, this was supported by a strong correlation between PIC and both particulate backscattering (r = 0.81, p < 0.005) and particulate beam attenuation coefficient (r = 0.7, p < 0.05). Remote sensing reflectance data were strongly related to particle backscattering and backscattering ratio, but not to absorption. NASA operational algorithms overestimated chlorophyll by a factor of similar to 2 and estimated PIC with a relatively high root-mean-square (RMS) error (RMS = 97.9 mu g PIC L-1). Better estimates of PIC values (RMS = 81.5 mu g PIC L-1) were achieved when we used the original PIC-specific backscattering coefficient (Balch et al., 2005).
C1 [Eiras Garcia, Carlos Alberto; Tavano Garcia, Virginia Maria; Ferreira, Amabile; Souza, Marcio S.; Mata, Mauricio M.] Univ Fed Rio Grande, Inst Oceanog, Rio Grande, Brazil.
[Dogliotti, Ana Ines] Ciudad Sanitaria & Univ Vall Hebron, Inst Astron Fis Espacio, Buenos Aires, DF, Argentina.
[Romero, Silvia I.] Serv Hidrog Naval, Buenos Aires, DF, Argentina.
[Mannino, Antonio] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Garcia, CAE (reprint author), Univ Fed Rio Grande, Inst Oceanog, Rio Grande, Brazil.
RI Tavano, Virginia/C-5241-2013; Ferreira, Amabile /H-8245-2013; Mannino,
Antonio/I-3633-2014; Garcia, Carlos/K-7382-2012; Mata,
Mauricio/H-4605-2011
OI de Souza, Marcio Silva/0000-0003-1572-9307; Tavano,
Virginia/0000-0003-0039-8111; Romero, Silvia Ines/0000-0001-7744-6391;
Mata, Mauricio/0000-0002-9028-8284
FU Ministry of Science and Technology (MCT); CNPq (Brazilian National
Council on Research and Development) [520189/2006-0]; GSFC/NASA
[OCEANS/04123400362]
FX The Patagonian Experiment (PATEX) is a multidisciplinary project part of
the Group of High Latitude Oceanography (GOAL) activities in the
Brazilian Antarctic Program. We thank the crew of the Brazilian Navy RV
Ary Rongel for their assistance during the field sampling. We also
acknowledge the Servicio de Hidrografia Naval (Argentina) for their
cooperation in obtaining clearance for carrying out field work within
Argentinean EEZ. We thank Michael Novak at NASA/GSFC for analyzing the
POC and PIC samples. The cruise PATEX 5 was conducted under the umbrella
of the project "Southern Ocean Studies for Understanding Climate Changes
Issues" (SOS-CLIMATE), a Brazilian contribution to the International
Polar Year. We would like to thank two anonymous reviewers whose
criticisms and suggestions have improved this manuscript. The project
was sponsored through the funding resources of Ministry of Science and
Technology (MCT) and CNPq (Brazilian National Council on Research and
Development, grant 520189/2006-0) to the Brazilian Antarctic Program
(PROANTAR). This work was partly supported by GSFC/NASA through the
project OCEANS/04123400362. Ocean color images were provided by and
processed at the Goddard Space Flight Center (GSFC).
NR 63
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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 MAR 25
PY 2011
VL 116
AR C03025
DI 10.1029/2010JC006595
PG 17
WC Oceanography
SC Oceanography
GA 741LZ
UT WOS:000288866500001
ER
PT J
AU Simionescu, A
Allen, SW
Mantz, A
Werner, N
Takei, Y
Morris, RG
Fabian, AC
Sanders, JS
Nulsen, PEJ
George, MR
Taylor, GB
AF Simionescu, Aurora
Allen, Steven W.
Mantz, Adam
Werner, Norbert
Takei, Yoh
Morris, R. Glenn
Fabian, Andrew C.
Sanders, Jeremy S.
Nulsen, Paul E. J.
George, Matthew R.
Taylor, Gregory B.
TI Baryons at the Edge of the X-ray-Brightest Galaxy Cluster
SO SCIENCE
LA English
DT Article
ID VIRIAL RADIUS; INTRACLUSTER MEDIUM; MASS FRACTION; DARK ENERGY; SUZAKU;
CONSTRAINTS; TEMPERATURE; ENTROPY; PROFILE; DENSITY
AB Studies of the diffuse x-ray-emitting gas in galaxy clusters have provided powerful constraints on cosmological parameters and insights into plasma astrophysics. However, measurements of the faint cluster outskirts have become possible only recently. Using data from the Suzaku x-ray telescope, we determined an accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of the Perseus Cluster. Contrary to previous results, our measurements of the cluster baryon fraction are consistent with the expected universal value at half of the virial radius. The apparent baryon fraction exceeds the cosmic mean at larger radii, suggesting a clumpy distribution of the gas, which is important for understanding the ongoing growth of clusters from the surrounding cosmic web.
C1 [Simionescu, Aurora; Allen, Steven W.; Werner, Norbert; Morris, R. Glenn] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Mantz, Adam] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Takei, Yoh] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Fabian, Andrew C.; Sanders, Jeremy S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Nulsen, Paul E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Taylor, Gregory B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Taylor, Gregory B.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Simionescu, A (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA.
EM asimi@stanford.edu
RI XRAY, SUZAKU/A-1808-2009;
OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493
FU NASA [PF9-00070, PF8-90056, NAS8-03060, NNX09AV64G, NNX10AR48G,
NNX08AZ88G]; JAXA; U.S. Department of Energy [DE-AC02-76SF00515];
Ministry of Education, Culture, Sports, Science, and Technology of Japan
[22111513]; Chandra award [GO0-11138B]
FX We thank P. Thomas and O. Young for kindly providing the simulation
results shown in Fig. 4. Support for this work was provided by NASA
through Einstein Postdoctoral Fellowship grants number PF9-00070 and
PF8-90056 awarded by the Chandra X-ray Center, which is operated by the
Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. We acknowledge NASA grants NNX09AV64G and NNX10AR48G, issued
through the Suzaku Guest Observer program, and grant NNX08AZ88G. The
authors thank the Suzaku operation team and Guest Observer Facility,
supported by JAXA and NASA. This work was supported in part by the U.S.
Department of Energy under contract number DE-AC02-76SF00515. We also
acknowledge the Grant-in-Aid for Scientific Research of the Ministry of
Education, Culture, Sports, Science, and Technology of Japan (KAKENHI
no. 22111513) and Chandra award GO0-11138B.
NR 28
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U1 2
U2 6
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 MAR 25
PY 2011
VL 331
IS 6024
BP 1576
EP 1579
DI 10.1126/science.1200331
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 739XH
UT WOS:000288754500047
PM 21436446
ER
PT J
AU Bell, RE
Ferraccioli, F
Creyts, TT
Braaten, D
Corr, H
Das, I
Damaske, D
Frearson, N
Jordan, T
Rose, K
Studinger, M
Wolovick, M
AF Bell, Robin E.
Ferraccioli, Fausto
Creyts, Timothy T.
Braaten, David
Corr, Hugh
Das, Indrani
Damaske, Detlef
Frearson, Nicholas
Jordan, Thomas
Rose, Kathryn
Studinger, Michael
Wolovick, Michael
TI Widespread Persistent Thickening of the East Antarctic Ice Sheet by
Freezing from the Base
SO SCIENCE
LA English
DT Article
ID LAKE VOSTOK
AB An International Polar Year aerogeophysical investigation of the high interior of East Antarctica reveals widespread freeze-on that drives substantial mass redistribution at the bottom of the ice sheet. Although the surface accumulation of snow remains the primary mechanism for ice sheet growth, beneath Dome A, 24% of the base by area is frozen-on ice. In some places, up to half of the ice thickness has been added from below. These ice packages result from the conductive cooling of water ponded near the Gamburtsev Subglacial Mountain ridges and the supercooling of water forced up steep valley walls. Persistent freeze-on thickens the ice column, alters basal ice rheology and fabric, and upwarps the overlying ice sheet, including the oldest atmospheric climate archive, and drives flow behavior not captured in present models.
C1 [Bell, Robin E.; Creyts, Timothy T.; Das, Indrani; Frearson, Nicholas; Wolovick, Michael] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Ferraccioli, Fausto; Corr, Hugh; Jordan, Thomas; Rose, Kathryn] British Antarctic Survey, Cambridge CB3 0ET, England.
[Braaten, David] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
[Damaske, Detlef] Bundesanstalt Geowissensch & Rohstoffe, D-3000 Hannover, Germany.
[Studinger, Michael] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Studinger, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Bell, RE (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
EM robinb@ldeo.columbia.edu
RI Corr, Hugh/C-5398-2011;
OI Jordan, Tom/0000-0003-2780-1986
NR 13
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U1 3
U2 29
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 MAR 25
PY 2011
VL 331
IS 6024
BP 1592
EP 1595
DI 10.1126/science.1200109
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 739XH
UT WOS:000288754500052
PM 21385719
ER
PT J
AU Acikmese, B
Carson, JM
Bayard, DS
AF Acikmese, Behcet
Carson, John M., III
Bayard, David S.
TI A robust model predictive control algorithm for incrementally conic
uncertain/nonlinear systems
SO INTERNATIONAL JOURNAL OF ROBUST AND NONLINEAR CONTROL
LA English
DT Article
DE model predictive control; robust control; Lyapunov theory; nonlinear
systems; uncertain systems; linear matrix inequalities; receding horizon
control; incrementally conic uncertainty
ID RECEDING HORIZON CONTROL; CONSTRAINED LINEAR-SYSTEMS; STABILITY
AB This paper presents a robustly stabilizing model predictive control algorithm for systems with incrementally conic uncertain/nonlinear terms and bounded disturbances. The resulting control input consists of feedforward and feedback components. The feedforward control generates a nominal trajectory from online solution of a finite-horizon constrained optimal control problem for a nominal system model. The feedback control policy is designed off-line by utilizing a model of the uncertainty/nonlinearity and establishes invariant 'state tubes' around the nominal system trajectories. The entire controller is shown to be robustly stabilizing with a region of attraction composed of the initial states for which the finite-horizon constrained optimal control problem is feasible for the nominal system. Synthesis of the feedback control policy involves solution of linear matrix inequalities. An illustrative numerical example is provided to demonstrate the control design and the resulting closed-loop system performance. Copyright (C) 2010 John Wiley & Sons, Ltd.
C1 [Acikmese, Behcet; Carson, John M., III; Bayard, David S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Acikmese, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 198-326, Pasadena, CA 91109 USA.
EM behcet@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We gratefully acknowledge Daniel P. Scharf, Linh H. Phan, and Fred Y.
Hadaegh of JPL, Richard M. Murray and Douglas G. MacMynowski of
California Institute of Technology, and Roy S. Smith of University of
California, Santa Barbara, for their very valuable comments and
suggestions. We gratefully acknowledge Martin Corless of Purdue
University for the insight he provided into LMI analysis of nonlinear
systems. This research was performed at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 33
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U1 1
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1049-8923
EI 1099-1239
J9 INT J ROBUST NONLIN
JI Int. J. Robust Nonlinear Control
PD MAR 25
PY 2011
VL 21
IS 5
BP 563
EP 590
DI 10.1002/rnc.1613
PG 28
WC Automation & Control Systems; Engineering, Electrical & Electronic;
Mathematics, Applied
SC Automation & Control Systems; Engineering; Mathematics
GA 731HR
UT WOS:000288097400006
ER
PT J
AU Tanaka, I
De Breuck, C
Kurk, JD
Taniguchi, Y
Kodama, T
Matsuda, Y
Packham, C
Zirm, A
Kajisawa, M
Ichikawa, T
Seymour, N
Stern, D
Stockton, A
Venemans, BP
Vernet, J
AF Tanaka, Ichi
De Breuck, Carlos
Kurk, Jaron D.
Taniguchi, Yoshiaki
Kodama, Tadayuki
Matsuda, Yuichi
Packham, Chris
Zirm, Andrew
Kajisawa, Masaru
Ichikawa, Takashi
Seymour, Nick
Stern, Daniel
Stockton, Alan
Venemans, Bram P.
Vernet, Joel
TI Discovery of an Excess of H alpha Emitters around 4C 23.56 at z=2.48
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE galaxies: H alpha emitters; galaxies: high redshifts; galaxies:
individual (4C 23.56); galaxies: protocluster
ID COLOR-MAGNITUDE RELATION; EARLY-TYPE GALAXIES; STAR-FORMING GALAXIES;
XMM CLUSTER SURVEY; NEAR-INFRARED SPECTROSCOPY; FORMATION-DENSITY
RELATION; HIGH-REDSHIFT CLUSTERS; SPECTRUM RADIO-SOURCES; LARGE-SCALE
STRUCTURE; DIGITAL SKY SURVEY
AB We report on the discovery of a significant excess of candidate Ha emitters (HAEs) in the field of the radio galaxy 4C 23.56 at z = 2.483. Using the MOIRCS near-infrared imager on the Subaru Telescope we found 11 candidate emission-line galaxies to a flux limit of similar to 7.5 x 10(-17) erg s(-1) cm(-2), which is about 5-times excess from the expected field counts with an similar to 3-sigma significance. Three of these have been spectroscopically confirmed as redshifted H alpha at z = 2.49. The distribution of candidate emitters on the sky is tightly confined to a 1.2-Mpc-radius area at z = 2.49, locating 4C 23.56 at the western edge of the distribution. An analysis of the deep Spitzer MIPS 24 mu m imaging shows that there is also an excess of faint MIPS sources. All but two of the 11 HAEs are also found in the MIPS data. The inferred star-formation rate (SFR) of the HAEs based on the extinction-corrected H alpha luminosity (median SFR greater than or similar to 100 M-circle dot yr(-1)) is similar to those of HAEs in random fields at z similar to 2. On the other hand, the MIPS-based SFR for the HAEs is on average 3.6-times larger, suggesting the existence of star-formation significanly obscured by dust. A comparison of the H alpha-based star-formation activities of the HAEs in the 4C 23.56 field to those in another proto-cluster around PKS 1138-262 at z = 2.16 reveals that the latter tend to have fainter H alpha emission despite similar K-band magnitudes. This suggests that star-formation may be suppressed in the PKS 1138-262 protocluster relative to the 4C 23.56 protocluster This difference among the HAEs in the two proto-clusters at z > 2 may imply that some massive cluster galaxies are just forming at these epochs with some variation among them.
C1 [Tanaka, Ichi; Kodama, Tadayuki] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[De Breuck, Carlos; Venemans, Bram P.; Vernet, Joel] European So Observ, D-85748 Garching, Germany.
[Kurk, Jaron D.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Taniguchi, Yoshiaki] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Kodama, Tadayuki; Kajisawa, Masaru] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Matsuda, Yuichi] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Packham, Chris] Univ Florida, Dept Astron, Bryant Sci Ctr 211, Gainesville, FL 32611 USA.
[Zirm, Andrew] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Kajisawa, Masaru; Ichikawa, Takashi] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Seymour, Nick] UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stockton, Alan] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Tanaka, I (reprint author), Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
EM ichi@subaru.naoj.org
OI Vernet, Joel/0000-0002-8639-8560
FU JSPS; ESO; Ministry of Education, Culture, Sports, Science and
Technology in Japan [19340046, 21340045]; DFG [STE1869/1-1.GE625/15-1];
NASA
FX We thank an anonymous referee for comments that lead to improvements of
the paper. We thank the MOIRCS Deep Survey Team for providing us with
the MODS catalog. Also, we would like to thank Dr. Sune Toft and Dr.
Masa Tanaka, and many others for useful comments and suggestions. We
also thank Dr. Ryuji Suzuki for providing simulation data on the shift
of the central wavelength of NB filters. This work was supported by the
JSPS Institutional Program for Young Researcher Overseas Visits. This
work was also partly supported by the Visitor Programs by the ESO. YT
and TK thank for support via Grant-in-Aid for Scientific Research
(KAKENHI: Nos. 19340046 and 21340045, respectively) by the Ministry of
Education, Culture, Sports, Science and Technology in Japan. JK thanks
the DFG for support via German-Israeli Project Cooperation grant
STE1869/1-1.GE625/15-1. IT would like to thank the all ESO staff for the
hospitality during the stay in ESO Garching. IT would also like to thank
all staffs and members of the DARK Cosmology Center, MSSL University
College London, and Durham University for their warm hospitality during
my stay related to this study. This work is based on data collected at
Subaru Telescope, which is operated by the National Astronomical
Observatory of Japan. This 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, as well as the data collected by the 4.2 m William
Herschel Telescope which 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.
NR 153
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U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD MAR 25
PY 2011
VL 63
SI 2
BP S415
EP S435
DI 10.1093/pasj/63.sp2.S415
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 770GW
UT WOS:000291076000004
ER
PT J
AU Zeitlin, C
Miller, J
Guetersloh, S
Heilbronn, L
Fukumura, A
Iwata, Y
Murakami, T
Blattnig, S
Norman, R
Mashnik, S
AF Zeitlin, C.
Miller, J.
Guetersloh, S.
Heilbronn, L.
Fukumura, A.
Iwata, Y.
Murakami, T.
Blattnig, S.
Norman, R.
Mashnik, S.
TI Fragmentation of N-14, O-16, Ne-20, and Mg-24 nuclei at 290 to 1000
MeV/nucleon
SO PHYSICAL REVIEW C
LA English
DT Article
ID PRODUCTION CROSS-SECTIONS; PROJECTILE FRAGMENTATION; RELATIVISTIC
NUCLEI; CARBON TARGETS; HYDROGEN; CHARGE; PHITS; COLLISIONS; ENERGIES;
NUCFRG2
AB We report fragmentation cross sections measured at 0 degrees for beams of N-14, O-16, Ne-20, and Mg-24 ions, at energies ranging from 290 MeV/nucleon to 1000 MeV/nucleon. Beams were incident on targets of C, CH2, Al, Cu, Sn, and Pb, with the C and CH2 target data used to obtain hydrogen-target cross sections. Using methods established in earlier work, cross sections obtained with both large-acceptance and small-acceptance detectors are extracted from the data and, when necessary, corrected for acceptance effects. The large-acceptance data yield cross sections for fragments with charges approximately half of the beam charge and above, with minimal corrections. Cross sections for lighter fragments are obtained from small-acceptance spectra, with more significant, model-dependent corrections that account for the fragment angular distributions. Results for both charge-changing and fragment production cross sections are compared to the predictions of the Los Alamos version of the quark gluon string model (LAQGSM) as well as the NASA Nuclear Fragmentation (NUCFRG2) model and the Particle and Heavy Ion Transport System (PHITS) model. For all beams and targets, cross sections for fragments as light as He are compared to the models. Estimates of multiplicity-weighted helium production cross sections are obtained from the data and compared to PHITS and LAQGSM predictions. Summary statistics show that the level of agreement between data and predictions is slightly better for PHITS than for either NUCFRG2 or LAQGSM.
C1 [Zeitlin, C.] SW Res Inst, Boulder, CO 80302 USA.
[Miller, J.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Guetersloh, S.] Texas A&M Univ, Dept Nucl Engn, College Stn, TX 77843 USA.
[Heilbronn, L.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
[Fukumura, A.; Iwata, Y.; Murakami, T.] Natl Inst Radiol Sci, Chiba 260, Japan.
[Blattnig, S.; Norman, R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Mashnik, S.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Zeitlin, C (reprint author), SW Res Inst, Boulder, CO 80302 USA.
EM zeitlin@boulder.swri.edu
RI Heilbronn, Lawrence/J-6998-2013; Norman, Ryan/D-5095-2017
OI Heilbronn, Lawrence/0000-0002-8226-1057; Norman,
Ryan/0000-0002-9103-7225
FU NASA [NNX09AE18A]; National Aeronautics and Space Administration under
NASA [L14230C, H31909D]; US Department of Energy [DE-AC03076SF00098];
NIRS-HIMAC [P037]; Defense Threat Reduction Agency (DTRA)
[DE-AC52-06NA25396]
FX This work was supported at Southwest Research Institute by NASA Grant
No. NNX09AE18A. At LBNL, this work was supported by the Space Radiation
Health Program of the National Aeronautics and Space Administration
under NASA Grant Nos. L14230C and H31909D, through the US Department of
Energy under Contract No. DE-AC03076SF00098. At HIMAC, this work was
supported in part by the Research Project with Heavy Ions at NIRS-HIMAC,
Project No. P037. The part of this work performed at LANL was carried
out under the auspices of the National Nuclear Security Administration
of the US Department of Energy at Los Alamos National Laboratory under
Contract No. DE-AC52-06NA25396 with funding from the Defense Threat
Reduction Agency (DTRA).
NR 36
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U1 0
U2 11
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0556-2813
J9 PHYS REV C
JI Phys. Rev. C
PD MAR 24
PY 2011
VL 83
IS 3
AR 034909
DI 10.1103/PhysRevC.83.034909
PG 23
WC Physics, Nuclear
SC Physics
GA 740IO
UT WOS:000288786200004
ER
PT J
AU Ebihara, Y
Fok, MC
Immel, TJ
Brandt, PC
AF Ebihara, Y.
Fok, M. -C.
Immel, T. J.
Brandt, P. C.
TI Rapid decay of storm time ring current due to pitch angle scattering in
curved field line
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INNER MAGNETOSPHERE; GEOMAGNETIC STORMS; PLASMA SHEET; PROTON
PRECIPITATION; IMAGE SPACECRAFT; MAGNETIC STORMS; RECOVERY PHASE;
FEBRUARY 1986; CURRENT IONS; DISTRIBUTIONS
AB The storm time ring current sometimes exhibits rapid decay, as suggested from the Dst index, but the underlying mechanism is unknown. By means of a simulation with pitch angle scattering due to the field line curvature (FLC), together with the charge exchange and adiabatic loss cone loss, we investigated rapid decay of the storm time ring current for the large magnetic storm that occurred on 12 August 2000. When all three loss processes were included, the Dst (SYM-H) index showed rapid recovery with an e-folding time of similar to 6 h. However, without FLC scattering, the simulated Dst (SYM-H) index showed a slower recovery with an e-folding time of similar to 12 h. Overall flux of energetic neutral hydrogen with energy >= 39 keV was significantly reduced by the FLC scattering and is consistent with data from the high energy neutral analyzer (HENA) on board the IMAGE satellite. Power of precipitating protons showed a fairly good agreement with data from the far ultraviolet (FUV) imager on board IMAGE. These fairly good agreements with observations lead to the possible conclusion that the FLC scattering is a significant loss mechanism for the ring current ions, and the main oval of the proton aurora is likely a manifestation of the precipitating loss of the protons for this particular storm.
C1 [Ebihara, Y.] Nagoya Univ, Inst Adv Res, Aichi, Japan.
[Fok, M. -C.] NASA GSFC, Greenbelt, MD 20771 USA.
[Immel, T. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Ebihara, Y (reprint author), Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto 6110011, Japan.
EM ebihara@rish.kyoto-u.ac.jp
RI Fok, Mei-Ching/D-1626-2012; Ebihara, Yusuke/D-1638-2013; Brandt,
Pontus/N-1218-2016
OI Ebihara, Yusuke/0000-0002-2293-1557; Brandt, Pontus/0000-0002-4644-0306
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) of
Japan; Japan Society for the Promotion of Science (JSPS) [19340141]
FX The Dst index was provided by WDC Kyoto. The OMNI data were obtained
from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov/.
The authors thank Nikolai A. Tsyganenko for the empirical magnetic field
model and Daniel R. Weimer for the empirical convection electric field
model. The work of Y.E. is supported by the Program for Improvement of
Research Environment for Young Researchers from the Special Coordination
Funds for Promoting Science and Technology (SCF) commissioned by the
Ministry of Education, Culture, Sports, Science and Technology (MEXT) of
Japan. This study is also supported by a Grant-in-Aid for Young
Scientists (B) (19340141) by the Japan Society for the Promotion of
Science (JSPS).
NR 68
TC 8
Z9 8
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR 23
PY 2011
VL 116
AR A03218
DI 10.1029/2010JA016000
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 741OK
UT WOS:000288872800006
ER
PT J
AU Waliser, DE
Li, JLF
L'Ecuyer, TS
Chen, WT
AF Waliser, D. E.
Li, J. -L. F.
L'Ecuyer, T. S.
Chen, W. -T.
TI The impact of precipitating ice and snow on the radiation balance in
global climate models
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID PARTICLE TERMINAL VELOCITIES; CIRRUS CLOUDS
AB Climate models often ignore the radiative impact of precipitating hydrometeors. CloudSat retrievals provide the first means to distinguish between cloud versus precipitating ice mass and characterize its vertical structure. With this information, radiative transfer calculations are performed to examine the impact of excluding precipitating ice on atmospheric radiative fluxes and heating rates. The preliminary results show that such exclusion can result in underestimates of the reflective shortwave flux at the top of the atmosphere (TOA) and overestimates of the downwelling surface shortwave and emitted TOA longwave flux, with the differences being about 5-10 Wm(-2) in the most convective and rainfall intensive areas and greatest for the TOA longwave flux. There are also considerable differences (similar to 10-25%) in the vertical profiles of shortwave and longwave heating, resulting in an overestimation (similar to up to 10%) of the integrated column cooling. The implications of these results are that models that exclude these ice components are achieving TOA radiation balance through compensating errors as well as possibly introducing biases in atmospheric circulations. Citation: Waliser, D. E., J.-L. F. Li, T. S. L'Ecuyer, and W.-T. Chen (2011), The impact of precipitating ice and snow on the radiation balance in global climate models, Geophys. Res. Lett., 38, L06802, doi: 10.1029/2010GL046478.
C1 [Waliser, D. E.; Li, J. -L. F.; Chen, W. -T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[L'Ecuyer, T. S.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
RP Waliser, DE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM duane.waliser@jpl.nasa.gov
RI L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer, Tristan/E-5607-2012; Chen,
Wei-Ting/A-4476-2012
OI L'Ecuyer, Tristan/0000-0002-7584-4836; Chen,
Wei-Ting/0000-0002-9292-0933
FU NASA
FX We would like to thank Yuk Yung, King-Fai Li, and Lazaros Oreopoulos for
reading and providing comments on the manuscript. The contributions by
DEW, JLL and WTC were carried out on behalf of the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. TSL was supported by
the NASA NEWS and CloudSats projects. TSL would like to thank Phil
Partain at the CloudSat Data Processing Center for assistance in running
the revised FLXHR calculations.
NR 14
TC 30
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U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 23
PY 2011
VL 38
AR L06802
DI 10.1029/2010GL046478
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 741LD
UT WOS:000288864300002
ER
PT J
AU Alexander, SP
Klekociuk, AR
Pitts, MC
McDonald, AJ
Arevalo-Torres, A
AF Alexander, S. P.
Klekociuk, A. R.
Pitts, M. C.
McDonald, A. J.
Arevalo-Torres, A.
TI The effect of orographic gravity waves on Antarctic polar stratospheric
cloud occurrence and composition
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID NITRIC-ACID TRIHYDRATE; MOUNTAIN WAVES; ARCTIC STRATOSPHERE; OZONE
DEPLETION; DENITRIFICATION; MICROPHYSICS; CHEMISTRY; SATELLITE; CALIPSO;
SYSTEM
AB A seasonal analysis of the relationship between mesoscale orographic gravity wave activity and polar stratospheric cloud (PSC) composition occurrence around the whole of Antarctica is presented. Gravity wave variances are derived from temperature measurements made with the Constellation Observing System for Meteorology, Ionosphere and Climate (COSMIC) Global Positioning System Radio Occultation (GPS-RO) satellites. Data from the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) instrument onboard the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite are used to determine the PSC composition class distribution and spatial volume. The results show intermittent large wave activity above the Antarctic Peninsula which is coincident with large volumes of H2O ice PSCs. These ice PSC volumes advect downstream, where increases in nitric acid trihydrate (NAT) PSC volumes occur, supporting the mountain wave seeding hypothesis. During winter 2007 in the latitude range 60 degrees S-70 degrees S, near the edge of the vortex and where temperatures are close to PSC formation thresholds, 30% of all PSCs are attributable to orographic gravity waves. In the separate composition classes, around 50% of both H2O ice PSCs and a high NAT number density liquid-NAT mixture class of PSCs are due to these waves. While we show that planetary waves are the major determinant of PSC presence at temperatures close to the NAT formation threshold, we also demonstrate the important role of mesoscale, intermittent orographic gravity wave activity in accounting for the composition and distribution of PSCs around Antarctica.
C1 [Alexander, S. P.; Klekociuk, A. R.] Australian Antarctic Div, Kingston, Tas 7050, Australia.
[Pitts, M. C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[McDonald, A. J.; Arevalo-Torres, A.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
RP Alexander, SP (reprint author), Australian Antarctic Div, 203 Channel Hwy, Kingston, Tas 7050, Australia.
EM simon.alexander@aad.gov.au
RI Klekociuk, Andrew/A-4498-2015;
OI Klekociuk, Andrew/0000-0003-3335-0034; Alexander,
Simon/0000-0001-6823-8857; McDonald, Adrian/0000-0002-1456-6254
FU Antarctica New Zealand; University of Canterbury; SEP-DRGI
FX The CALIPSO CALIOP v2.01 level 1B profile data products were obtained
through the NASA Langley Atmospheric Science Data Center (ASDC). The
COSMIC version 2.0 dry temperature data from the COSMIC Data Analysis
and Archive Center (CDAAC). Aura MLS data used in this study were
acquired as part of NASA's Earth-Sun System Division and archived and
distributed by the Goddard Earth Sciences (GES) Data and Information
Services Center (DISC) Distributed Active Archive Center (DAAC). This
research was conducted for projects 737 and 3140 of the Australian
Antarctic program and partially supported by Antarctica New Zealand. One
of the authors (A.A.-T.) is supported under a University of Canterbury
and SEP-DRGI postgraduate research fund. We thank three anonymous
reviewers for their valuable comments on an earlier version of this
manuscript.
NR 57
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U1 2
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 23
PY 2011
VL 116
AR D06109
DI 10.1029/2010JD015184
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 741LR
UT WOS:000288865700003
ER
PT J
AU Liang, CK
Eldering, A
Gettelman, A
Tian, B
Wong, S
Fetzer, EJ
Liou, KN
AF Liang, C. K.
Eldering, A.
Gettelman, A.
Tian, B.
Wong, S.
Fetzer, E. J.
Liou, K. N.
TI Record of tropical interannual variability of temperature and water
vapor from a combined AIRS-MLS data set
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; INFRARED SOUNDER TEMPERATURE; LOWER
STRATOSPHERE; SURFACE-TEMPERATURE; NCEP REANALYSES; DEEP CONVECTION;
TROPOPAUSE; CIRCULATION; VALIDATION; ATMOSPHERE
AB We utilize a merged AIRS and MLS temperature and water vapor record (August 2004 to March 2010) to study the atmospheric variability of these quantities. The seasonal and spatial distribution of temperature and humidity shows the tropical western Pacific (TWP, 8 degrees S-8 degrees N, 120 degrees E-170 degrees E) to be a location with persistent deep convection and the tropical central Pacific (TCP, 8 degrees S-8 degrees N, 120 degrees W-170 degrees W) to be a region of subsidence, consistent with previous work. Furthermore, our estimates of 3.9 +/- 0.3 ppmv and 4.9 +/- 0.9 ppmv for the tropical mean stratospheric entry water vapor concentration and saturation mixing ratio, respectively, are well within previous estimates from a wide variety of observations. We also find that the interannual variability modes of the El Nino-Southern Oscillation (ENSO) and the quasi-biennial oscillation (QBO) both impact the tropopause region. The TWP (TCP) experiences enhancements (cancellation) of temperature anomalies when the ENSO and QBO are in phase. When these interannual modes fall out of phase the additive behavior of the anomalies migrate to the TCP with the TWP experiencing weaker anomalies. In both cases a change in the water vapor distribution is also observed. Our results are consistent with previous results, showing that this migration of anomaly enhancement and cancellation is a result of the ENSO impact on the Walker Circulation and the period when this occurs relative to the phase of the QBO. Our findings suggest that when the ENSO and QBO are out of phase, the TCP water vapor distribution may have a substantial impact on the tropical zonal water vapor distribution.
C1 [Liang, C. K.; Liou, K. N.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Liang, C. K.; Liou, K. N.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Eldering, A.; Tian, B.; Wong, S.; Fetzer, E. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gettelman, A.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
RP Liang, CK (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM cliang@atmos.ucla.edu; annmarie.eldering@jpl.nasa.gov; andrew@ucar.edu;
baijun.tian@jpl.nasa.gov; sun.wong@jpl.nasa.gov;
eric.j.fetzer@jpl.nasa.gov; knliou@atmos.ucla.edu
RI Tian, Baijun/A-1141-2007
OI Tian, Baijun/0000-0001-9369-2373
FU NASA Earth and Space Science [NNX09AO04H]; Northrop Grumman fellowship
FX C. K. Liang would like to thank H. Nguyen for helpful discussion on
determining statistical significance for remote sensing time series
records. The authors would also like to thank W. J. Randel for helpful
discussion on aspects of the QBO. C. K. Liang was supported by a NASA
Earth and Space Science Fellowship (NNX09AO04H) and Northrop Grumman
fellowship. AIRS and MLS data were obtained through the Goddard Earth
Sciences Data and Information Services Center
(http://daac.gsfc.nasa.gov/). This work was performed at the Jet
Propulsion Laboratory, California Institute of Technology.
NR 59
TC 18
Z9 18
U1 0
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 23
PY 2011
VL 116
AR D06103
DI 10.1029/2010JD014841
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 741LR
UT WOS:000288865700001
ER
PT J
AU Bahadori, AA
Van Baalen, M
Shavers, MR
Dodge, C
Semones, EJ
Bolch, WE
AF Bahadori, Amir A.
Van Baalen, Mary
Shavers, Mark R.
Dodge, Charles
Semones, Edward J.
Bolch, Wesley E.
TI The effect of anatomical modeling on space radiation dose estimates: a
comparison of doses for NASA phantoms and the 5th, 50th, and 95th
percentile male and female astronauts
SO PHYSICS IN MEDICINE AND BIOLOGY
LA English
DT Article
ID DEEP SPACE; EQUIVALENTS; DOSIMETRY; STATION
AB The National Aeronautics and Space Administration (NASA) performs organ dosimetry and risk assessment for astronauts using model-normalized measurements of the radiation fields encountered in space. To determine the radiation fields in an organ or tissue of interest, particle transport calculations are performed using self-shielding distributions generated with the computer program CAMERA to represent the human body. CAMERA mathematically traces linear rays (or path lengths) through the computerized anatomical man (CAM) phantom, a computational stylized model developed in the early 1970s with organ and body profiles modeled using solid shapes and scaled to represent the body morphometry of the 1950 50th percentile (PCTL) Air Force male. With the increasing use of voxel phantoms in medical and health physics, a conversion from a mathematical-based to a voxel-based ray-tracing algorithm is warranted. In this study, the voxel-based ray tracer (VoBRaT) is introduced to ray trace voxel phantoms using a modified version of the algorithm first proposed by Siddon (1985 Med. Phys. 12 252-5). After validation, VoBRAT is used to evaluate variations in body self-shielding distributions for NASA phantoms and six University of Florida (UF) hybrid phantoms, scaled to represent the 5th, 50th, and 95th PCTL male and female astronaut body morphometries, which have changed considerably since the inception of CAM. These body self-shielding distributions are used to generate organ dose equivalents and effective doses for five commonly evaluated space radiation environments. It is found that dosimetric differences among the phantoms are greatest for soft radiation spectra and light vehicular shielding.
C1 [Bahadori, Amir A.; Bolch, Wesley E.] Univ Florida, Dept Nucl & Radiol Engn, Gainesville, FL 32611 USA.
[Van Baalen, Mary; Semones, Edward J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Shavers, Mark R.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA.
[Dodge, Charles] Univ Houston Downtown, Houston, TX 77002 USA.
[Bolch, Wesley E.] Univ Florida, Dept Biomed Engn, Gainesville, FL 32611 USA.
RP Bolch, WE (reprint author), Univ Florida, Dept Nucl & Radiol Engn, Gainesville, FL 32611 USA.
EM wbolch@ufl.edu
FU NASA GSRP [NNX09AK14H]
FX This work was supported by NASA GSRP Grant NNX09AK14H.
NR 38
TC 8
Z9 9
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0031-9155
J9 PHYS MED BIOL
JI Phys. Med. Biol.
PD MAR 21
PY 2011
VL 56
IS 6
BP 1671
EP 1694
DI 10.1088/0031-9155/56/6/010
PG 24
WC Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Radiology, Nuclear Medicine & Medical Imaging
GA 728BK
UT WOS:000287848600010
PM 21346276
ER
PT J
AU Tada, S
Shen, Y
Jacqmin, D
Fu, BM
Qiu, ZY
AF Tada, Shigeru
Shen, Yan
Jacqmin, David
Fu, Bingmei
Qiu, Zhiyong
TI UNDERSTANDING ELECTRIC INTERACTIONS IN SUSPENSIONS IN GRADIENT AC
ELECTRIC FIELDS II: SIMULATIONS AND APPLICATION EXPLORATION
SO INTERNATIONAL JOURNAL OF MODERN PHYSICS B
LA English
DT Article
AB We used numerical simulations of a continuous model and the molecular dynamics model to understand the particle instability, formation of island like structures and existence of one critical particle concentration of 1% (v/v) for formation of is structures in the suspension in a gradient AC electric field reported in Paper I. The simulations of the continuous model show that the critical concentration of 1% (v/v) is the concentration of which the particles of a suspension are just fully filling the lower field region finally. According to the MD simulations, the particles instability does exist in the corn oil in a gradient AC electric field, anisotropic polarization interactions among the particles are responsible for the particle instability and have memory, and the memory is still kept even when the particles are transported by a dielectrophoresis force. The island-like structures can be regarded as signature of the memory. We explored possibilities to apply our findings in biomedical fields.
C1 [Fu, Bingmei; Qiu, Zhiyong] New York Ctr Biomed Engn, New York, NY 10031 USA.
[Fu, Bingmei; Qiu, Zhiyong] CUNY City Coll, New York, NY 10031 USA.
[Tada, Shigeru] Natl Def Acad, Kanagawa 2398686, Japan.
[Shen, Yan] Zhengzhou Univ Light Ind, Zhengzhou 450002, Henan, Peoples R China.
[Jacqmin, David] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Qiu, ZY (reprint author), New York Ctr Biomed Engn, 140th St & Convent Ave, New York, NY 10031 USA.
EM ltscltsc@hotmail.com
FU NASA [NAG3-2698]; PSC-CUNY
FX The authors gratefully acknowledged that this work was in part supported
by NASA under Grant No NAG3-2698 and PSC-CUNY Professional Development
Fund. The authors thank Dr. Junjun Mao for providing them with computing
resources of the Levich Institute of the City College of the City
University of New York for the MD simulations. The continuous model
simulations were conducted in NASA Glenn Research Center.
NR 5
TC 1
Z9 1
U1 0
U2 1
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE
SN 0217-9792
J9 INT J MOD PHYS B
JI Int. J. Mod. Phys. B
PD MAR 20
PY 2011
VL 25
IS 7
BP 927
EP 933
DI 10.1142/S0217979211058493
PG 7
WC Physics, Applied; Physics, Condensed Matter; Physics, Mathematical
SC Physics
GA 757PW
UT WOS:000290101200005
ER
PT J
AU Heckman, TM
Borthakuri, S
Overzier, R
Kauffmann, G
Basu-Zych, A
Leitherer, C
Sembach, K
Martin, DC
Rich, RM
Schiminovich, D
Seibert, M
AF Heckman, Timothy M.
Borthakuri, Sanchayeeta
Overzier, Roderik
Kauffmann, Guinevere
Basu-Zych, Antara
Leitherer, Claus
Sembach, Ken
Martin, D. Chris
Rich, R. Michael
Schiminovich, David
Seibert, Mark
TI EXTREME FEEDBACK AND THE EPOCH OF REIONIZATION: CLUES IN THE LOCAL
UNIVERSE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: ISM; galaxies:
kinematics and dynamics; intergalactic medium
ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; ULTRAVIOLET-LUMINOUS
GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; GRAVITATIONALLY LENSED
GALAXY; DRIVEN GALACTIC SUPERWINDS; CONTINUUM ESCAPE FRACTION;
SPACE-TELESCOPE SEARCH; X-RAY OBSERVATIONS; SIMILAR-TO 3
AB The source responsible for reionizing the universe at z > 6 remains uncertain. While an energetically adequate population of star-forming galaxies may be in place, it is unknown whether a large enough fraction of their ionizing radiation can escape into the intergalactic medium. Attempts to measure this escape fraction in intensely star-forming galaxies at lower redshifts have largely yielded upper limits In this paper, we present new Hubble Space Telescope Cosmic Origins Spectrograph and archival Far-Ultraviolet Spectroscopic Explorer (FUSE) far-UV spectroscopy of a sample of 11 Lyman Break Analogs (LBAs), a rare population of local galaxies that strongly resemble the high-z Lyman Break galaxies. We combine these data with Sloan Digital Sky Survey optical spectra and Spitzer photometry. We also analyze archival FUSE observations of 15 typical UV-bright local starbursts. We find evidence of small covering factors for optically thick neutral gas in three cases. This is based on two independent pieces of evidence: a significant residual intensity in the cores of the strongest interstellar absorption-lines tracing neutral gas and a small ratio of extinction-corrected H alpha to UV plus far-IR luminosities. These objects represent three of the four LBAs that contain a young, very compact (similar to 10(2) pc), and highly massive (similar to 10(9) M-circle dot) dominant central object (DCO). These three objects also differ from the other galaxies in showing a significant amount of blueshifted Ly alpha emission, which may be related to the low covering factor of neutral gas. All four LBAs with DCOs in our sample show extremely high velocity outflows of interstellar gas, with line centroids blueshifted by about 700 km s(-1) and maximum outflow velocities reaching at least 1500 km s(-1). We show that these properties are consistent with an outflow driven by a powerful starburst that is exceptionally compact. We speculate that such extreme feedback may be required to enable the escape of ionizing radiation from star-forming galaxies.
C1 [Heckman, Timothy M.; Borthakuri, Sanchayeeta] Johns Hopkins Univ, Ctr Astrophys Sci, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Overzier, Roderik; Kauffmann, Guinevere] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Basu-Zych, Antara] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leitherer, Claus; Sembach, Ken] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Martin, D. Chris] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Seibert, Mark] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
RP Heckman, TM (reprint author), Johns Hopkins Univ, Ctr Astrophys Sci, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM heckman@pha.jhu.edu
FU NASA [NAS 5-26555]
FX Based on observations with the NASA/ESA Hubble Space Telescope, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555. The observations are associated
with GO programs 10920, 11107, and 11727.
NR 84
TC 97
Z9 97
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2011
VL 730
IS 1
AR 5
DI 10.1088/0004-637X/730/1/5
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735XI
UT WOS:000288453600005
ER
PT J
AU Katsuda, S
Tsunemi, H
Mori, K
Uchida, H
Kosugi, H
Kimura, M
Nakajima, H
Takakura, S
Petre, R
Hewitt, JW
Yamaguchi, H
AF Katsuda, Satoru
Tsunemi, Hiroshi
Mori, Koji
Uchida, Hiroyuki
Kosugi, Hiroko
Kimura, Masashi
Nakajima, Hiroshi
Takakura, Satoru
Petre, Robert
Hewitt, John W.
Yamaguchi, Hiroya
TI POSSIBLE CHARGE-EXCHANGE X-RAY EMISSION IN THE CYGNUS LOOP DETECTED WITH
SUZAKU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atomic processes; ISM: abundances; ISM: individual objects (Cygnus
Loop); ISM: supernova remnants; X-rays: ISM
ID SUPERNOVA REMNANT 1E-0102.2-7219; XMM-NEWTON OBSERVATION; SOLAR-WIND;
ABUNDANCE INHOMOGENEITY; NORTHEASTERN RIM; CHANDRA OBSERVATIONS;
INTERSTELLAR-MEDIUM; PLASMA STRUCTURE; BACKGROUND MAPS; GALACTIC DISK
AB X-ray spectroscopic measurements of the Cygnus Loop supernova remnant indicate that metal abundances throughout most of the remnant's rim are depleted to similar to 0.2 times the solar value. However, recent X-ray studies have revealed in some narrow regions along the outermost rim anomalously "enhanced" abundances (up to similar to 1 solar). The reason for these anomalous abundances is not understood. Here, we examine X-ray spectra in annular sectors covering nearly the entire rim of the Cygnus Loop using Suzaku (21 pointings) and XMM-Newton (1 pointing). We find that spectra in the "enhanced" abundance regions commonly show a strong emission feature at similar to 0.7 keV. This feature is likely a complex of He-like O K(gamma + delta + epsilon), although other possibilities cannot be fully excluded. The intensity of this emission relative to He-like O K alpha appears to be too high to be explained as thermal emission. This fact, as well as the spatial concentration of the anomalous abundances in the outermost rim, leads us to propose an origin from charge-exchange processes between neutrals and H-like O. We show that the presence of charge-exchange emission could lead to the inference of apparently "enhanced" metal abundances using pure thermal emission models. Accounting for charge-exchange emission, the actual abundances could be uniformly low throughout the rim. The overall abundance depletion remains an open question.
C1 [Katsuda, Satoru; Petre, Robert; Hewitt, John W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tsunemi, Hiroshi; Uchida, Hiroyuki; Kosugi, Hiroko; Kimura, Masashi; Nakajima, Hiroshi; Takakura, Satoru] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys, Miyazaki 8892192, Japan.
[Yamaguchi, Hiroya] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan.
RP Katsuda, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Satoru.Katsuda@nasa.gov
RI XRAY, SUZAKU/A-1808-2009
FU JSPS; NASA [NNG06EO90A]
FX The authors are grateful to Una Hwang and the anonymous referee for
numerous constructive and insightful comments which significantly
improved the quality of this paper. S.K. is supported by a JSPS Research
Fellowship for Research Abroad, and in part by the NASA grant under the
contract NNG06EO90A. M.K. is supported by a JSPS Research Fellowship for
Young Scientists.
NR 72
TC 23
Z9 23
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2011
VL 730
IS 1
AR 24
DI 10.1088/0004-637X/730/1/24
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735XI
UT WOS:000288453600024
ER
PT J
AU Pandian, JD
Momjian, E
Xu, Y
Menten, KM
Goldsmith, PF
AF Pandian, J. D.
Momjian, E.
Xu, Y.
Menten, K. M.
Goldsmith, P. F.
TI THE ARECIBO METHANOL MASER GALACTIC PLANE SURVEY. IV. ACCURATE
ASTROMETRY AND SOURCE MORPHOLOGIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; instrumentation: high angular resolution; masers; stars:
formation
ID VLBA CALIBRATOR SURVEY; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS;
HIGH-RESOLUTION; EMISSION; W3(OH); SITES; DISC
AB We present accurate absolute astrometry of 6.7 GHz methanol masers detected in the Arecibo Methanol Maser Galactic Plane Survey using MERLIN and the Expanded Very Large Array (EVLA). We estimate the absolute astrometry to be accurate to better than 15 and 80 mas for the MERLIN and EVLA observations, respectively. We also derive the morphologies of the maser emission distributions for sources stronger than similar to 1 Jy. The median spatial extent along the major axis of the regions showing maser emission is similar to 775 AU. We find a majority of methanol maser morphologies to be complex with some sources previously determined to have regular morphologies in fact being embedded within larger structures. This suggests that some maser spots do not have a compact core, which leads to them being resolved in high angular resolution observations. This also casts doubt on interpretations of the origin of methanol maser emission solely based on source morphologies. We also investigate the association of methanol masers with mid-infrared emission and find very close correspondence between methanol masers and 24 p,m point sources. This adds further credence to theoretical models that predict methanol masers to be pumped by warm dust emission and firmly reinforces the finding that Class II methanol masers are unambiguous tracers of embedded high-mass protostars.
C1 [Pandian, J. D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Momjian, E.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
[Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pandian, JD (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM jpandian@ifa.hawaii.edu
RI Goldsmith, Paul/H-3159-2016
FU Chinese NSF [NSF 11073054, NSF 10673024, NSF 10733030, NSF 10703010, NSF
10621303]; NBRPC [2007CB815403]; European Community [R113CT 2003
5058187]
FX We are grateful to Anita Richards for invaluable help in MERLIN data
processing and other useful discussions. We also thank Rob Beswick and
Peter Thomasson for their assistance in MERLIN data reduction, Anna
Bartkiewicz for useful discussion, and Jim Caswell whose comments helped
improve the paper. Y.X. was supported by the Chinese NSF through grants
NSF 11073054, NSF 10673024, NSF 10733030, NSF 10703010, and NSF
10621303, and NBRPC (973 Program) under grant 2007CB815403. This work
has benefited from research funding from the European Community's sixth
Framework Programme under RadioNet R113CT 2003 5058187. This work was
carried out in part by the Jet Propulsion Laboratory, California
Institute of Technology. This research has made use of NASA's
Astrophysics Data System.
NR 35
TC 19
Z9 19
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2011
VL 730
IS 1
AR 55
DI 10.1088/0004-637X/730/1/55
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735XI
UT WOS:000288453600054
ER
PT J
AU Petric, AO
Armus, L
Howell, J
Chan, B
Mazzarella, JM
Evans, AS
Surace, JA
Sanders, D
Appleton, P
Charmandaris, V
Diaz-Santos, T
Frayer, D
Haan, S
Inami, H
Iwasawa, K
Kim, D
Madore, B
Marshall, J
Spoon, H
Stierwalt, S
Sturm, E
U, V
Vavilkin, T
Veilleux, S
AF Petric, A. O.
Armus, L.
Howell, J.
Chan, B.
Mazzarella, J. M.
Evans, A. S.
Surace, J. A.
Sanders, D.
Appleton, P.
Charmandaris, V.
Diaz-Santos, T.
Frayer, D.
Haan, S.
Inami, H.
Iwasawa, K.
Kim, D.
Madore, B.
Marshall, J.
Spoon, H.
Stierwalt, S.
Sturm, E.
U, V.
Vavilkin, T.
Veilleux, S.
TI MID-INFRARED SPECTRAL DIAGNOSTICS OF LUMINOUS INFRARED GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: interactions
ID SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; POLYCYCLIC
AROMATIC-HYDROCARBONS; STAR-FORMATION HISTORY; SKY LIRG SURVEY;
STARBURST GALAXIES; OPTICAL SPECTROSCOPY; ENERGY-DISTRIBUTIONS; NEARBY
GALAXIES; 1ST-LOOK SURVEY
AB We present a statistical analysis of the mid-infrared (MIR) spectra of 248 luminous infrared (IR) galaxies (LIRGs) which comprise the Great Observatories All-sky LIRG Survey (GOALS) observed with the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. The GOALS sample enables a direct measurement of the relative contributions of star formation and active galactic nuclei (AGNs) to the total IR emission from a large sample of local LIRGs. The AGN contribution to the MIR emission (f(AGN)) is estimated by employing several diagnostics based on the properties of the [Ne v], [O IV], and [Ne II] fine-structure gas emission lines, the 6.2 mu m polycyclic aromatic hydrocarbon (PAH), and the shape of the MIR continuum. We find that 18% of all LIRGs contain an AGN and that in 10% of all sources the AGN contributes more than 50% of the total IR luminosity. Summing up the total IR luminosity contributed by AGNs in all our sources suggests that AGNs supply similar to 12% of the total energy emitted by LIRGs. The average spectrum of sources with an AGN looks similar to the average spectrum of sources without an AGN, but it has lower PAH emission and a flatter MIR continuum. AGN-dominated LIRGs have higher IR luminosities, warmer MIR colors, and are found in interacting systems more often than pure starburst LIRGs. However, we find no linear correlations between these properties and f(AGN). We used the IRAC colors of LIRGs to confirm that finding AGNs on the basis of their MIR colors may miss similar to 40% of AGN-dominated (U)LIRGs.
C1 [Petric, A. O.; Armus, L.; Howell, J.; Surace, J. A.; Haan, S.; Inami, H.; Marshall, J.; Stierwalt, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Chan, B.; Mazzarella, J. M.] CALTECH, Infrared Proc Ctr, Pasadena, CA 91125 USA.
[Evans, A. S.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Evans, A. S.; Kim, D.; U, V.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Sanders, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Appleton, P.] NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Charmandaris, V.; Diaz-Santos, T.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
[Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Iwasawa, K.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos ICC, E-08028 Barcelona, Spain.
[Iwasawa, K.] ICREA, Barcelona, Spain.
[Madore, B.] Carnegie Observ, Pasadena, CA 91101 USA.
[Spoon, H.] Cornell Univ, Ithaca, NY 14853 USA.
[Sturm, E.] MPE, D-85741 Garching, Germany.
[Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Petric, AO (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
RI Charmandaris, Vassilis/A-7196-2008;
OI Charmandaris, Vassilis/0000-0002-2688-1956; Mazzarella,
Joseph/0000-0002-8204-8619; Appleton, Philip/0000-0002-7607-8766
FU EU [ToK 39965, FP7-REGPOT 206469]; NASA [1407]; NASA through JPL/Caltech
FX We thank the anonymous referee for his comments which have significantly
improved our paper. V.C. acknowledges partial support from the EU grants
ToK 39965 and FP7-REGPOT 206469. A.P. thanks N. Flagey for multiple
readings of the document and comments which helped improve the clarity
of this text. A.P. also thanks V. Desai for help with the data analysis,
and C. Bridge for discussions and help with the merger classification of
the LIRGs in this paper.; This work is based primarily on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under NASA
contract 1407.; We have made use of the NASA/IPAC Extra-galactic
Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. Support
for this research was provided by NASA through an award issued by
JPL/Caltech.
NR 73
TC 83
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2011
VL 730
IS 1
AR 28
DI 10.1088/0004-637X/730/1/28
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735XI
UT WOS:000288453600028
ER
PT J
AU Kustu, MD
Fan, Y
Rodell, M
AF Kustu, M. Deniz
Fan, Ying
Rodell, Matthew
TI Possible link between irrigation in the US High Plains and increased
summer streamflow in the Midwest
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID MISSISSIPPI RIVER-BASIN; LAND-COVER CHANGE; UNITED-STATES; SPATIAL
CORRELATION; TRENDS; WATER; EVAPORATION; CLIMATE; ILLINOIS; IMPACTS
AB We have previously presented evidence that higher rates of evapotranspiration (ET) associated with irrigation in the U.S. High Plains has likely caused an increased downwind precipitation (P). July P over the Midwest increased by 20%-30% from the preirrigation period (1900-1950) to the postirrigation (1950-2000) period. In this study, we test the hypothesis that the increased July P has had hydrologic consequences, possibly increasing groundwater storage and streamflow. Seasonal analyses of hydrologic variables over Illinois suggest that the water table and streamflow response lags P - ET by 1-2 months, indicating August and September as the months when the increased July P may be detected. We analyzed long-term observations of water table depth at 10 wells in Illinois and streamflow at 46 gauges in Illinois-Ohio basins. The Mann-Kendal test for trends suggests field significant increases in groundwater storage and streamflow in August-September over the period of irrigation expansion. Examination of soil moisture response to present-day above-normal July P suggests that the increased July P can reach the water table in normal to wet years. Mann-Kendall tests suggest that there has been no change in pan evaporation and atmospheric vapor pressure deficit. This implies that soil water availability is the driver of changes in ET, and the increased P may have possibly increased ET. Other studies in the literature give further evidence of increased ET due to increased P. By ruling out a reduction in ET, we suggest that the observed increase in groundwater storage and streamflow in the Midwest is linked to the increased July precipitation attributed to High Plains irrigation. We note that the increases in late summer streamflow are rather small when placed in the context of seasonal dynamics, but they are conceptually important in that they point to a different cause of change.
C1 [Kustu, M. Deniz; Fan, Ying] Rutgers State Univ, Dept Earth & Planetary Sci, Wright Rieman Labs, Piscataway, NJ 08854 USA.
[Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Kustu, MD (reprint author), Rutgers State Univ, Dept Earth & Planetary Sci, Wright Rieman Labs, 610 Taylor Rd, Piscataway, NJ 08854 USA.
EM yingfan@rci.rutgers.edu
RI Rodell, Matthew/E-4946-2012
OI Rodell, Matthew/0000-0003-0106-7437
FU U.S. National Science Foundation [NSF-ATM-0450334]; U.S. Environmental
Protection Agency [EPA-STAR-R-834190]; Rutgers University [AEF2006-07]
FX Support comes from the U.S. National Science Foundation
(NSF-ATM-0450334), U.S. Environmental Protection Agency
(EPA-STAR-R-834190), and Rutgers University Academic Excellence Fund
(AEF2006-07). We thank Mathieu Gerbush and David Robinson at Rutgers
University Climate Lab for assisting us in obtaining climate data from
the archive at the National Climate Data Center. We also thank three
anonymous reviewers for their thoughtful comments and the editors for
their handling of the manuscript.
NR 45
TC 16
Z9 16
U1 3
U2 15
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 MAR 19
PY 2011
VL 47
AR W03522
DI 10.1029/2010WR010046
PG 21
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 737YN
UT WOS:000288606600001
ER
PT J
AU Crusius, J
Schroth, AW
Gasso, S
Moy, CM
Levy, RC
Gatica, M
AF Crusius, John
Schroth, Andrew W.
Gasso, Santiago
Moy, Christopher M.
Levy, Robert C.
Gatica, Myrna
TI Glacial flour dust storms in the Gulf of Alaska: Hydrologic and
meteorological controls and their importance as a source of bioavailable
iron
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB Iron is an essential micronutrient that limits primary productivity in much of the ocean, including the Gulf of Alaska (GoA). However, the processes that transport iron to the ocean surface are poorly quantified. We combine satellite and meteorological data to provide the first description of widespread dust transport from coastal Alaska into the GoA. Dust is frequently transported from glacially-derived sediment at the mouths of several rivers, the most prominent of which is the Copper River. These dust events occur most frequently in autumn, when coastal river levels are low and riverbed sediments are exposed. The dust plumes are transported several hundred kilometers beyond the continental shelf into iron-limited waters. We estimate the mass of dust transported from the Copper River valley during one 2006 dust event to be between 2580 ktons. Based on conservative estimates, this equates to a soluble iron loading of 30-200 tons. We suggest the soluble Fe flux from dust originating in glaciofluvial sediment deposits from the entire GoA coastline is two to three times larger, and is comparable to the annual Fe flux to GoA surface waters from eddies of coastal origin. Given that glaciers are retreating in the coastal GoA region and in other locations, it is important to examine whether fluxes of dust are increasing from glacierized landscapes to the ocean, and to assess the impact of associated Fe on marine ecosystems. Citation: Crusius, J., A. W. Schroth, S. Gasso, C. M. Moy, R. C. Levy, and M. Gatica (2011), Glacial flour dust storms in the Gulf of Alaska: Hydrologic and meteorological controls and their importance as a source of bioavailable iron, Geophys. Res. Lett., 38, L06602, doi: 10.1029/2010GL046573.
C1 [Crusius, John; Schroth, Andrew W.; Moy, Christopher M.] US Geol Survey, Woods Hole Coastal & Marine Sci Ctr, Woods Hole, MA 02543 USA.
[Gasso, Santiago] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Moy, Christopher M.] Univ Otago, Dept Geol, Dunedin 9054, New Zealand.
[Levy, Robert C.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Gatica, Myrna] CUNY Queens Coll, Sch Earth & Environm Sci, Flushing, NY 11367 USA.
RP Crusius, J (reprint author), US Geol Survey, Woods Hole Coastal & Marine Sci Ctr, 384 Woods Hole Rd, Woods Hole, MA 02543 USA.
EM jcrusius@usgs.gov
RI Levy, Robert/M-7764-2013; Gasso, Santiago/H-9571-2014
OI Levy, Robert/0000-0002-8933-5303; Gasso, Santiago/0000-0002-6872-0018
FU USGS CMGP; NCCWSC; Mendenhall postdoc program; Woods Hole PEP intern
program; NASA-IDS
FX We appreciate support from the USGS CMGP, NCCWSC, the Mendenhall postdoc
program, the Woods Hole PEP intern program, and from NASA-IDS. We thank
D. Eberl (USGS) for quantitative XRD data. We also thank J. Bargar and
J. Rogers at Stanford Synchrotron Radiation Light Source, run on behalf
of the DOE and E. Sholkovitz, D. Muhs, and two others for reviews.
NR 25
TC 48
Z9 49
U1 2
U2 28
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 MAR 18
PY 2011
VL 38
AR L06602
DI 10.1029/2010GL046573
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 737XV
UT WOS:000288604700004
ER
PT J
AU Mueller, B
Seneviratne, SI
Jimenez, C
Corti, T
Hirschi, M
Balsamo, G
Ciais, P
Dirmeyer, P
Fisher, JB
Guo, Z
Jung, M
Maignan, F
McCabe, MF
Reichle, R
Reichstein, M
Rodell, M
Sheffield, J
Teuling, AJ
Wang, K
Wood, EF
Zhang, Y
AF Mueller, B.
Seneviratne, S. I.
Jimenez, C.
Corti, T.
Hirschi, M.
Balsamo, G.
Ciais, P.
Dirmeyer, P.
Fisher, J. B.
Guo, Z.
Jung, M.
Maignan, F.
McCabe, M. F.
Reichle, R.
Reichstein, M.
Rodell, M.
Sheffield, J.
Teuling, A. J.
Wang, K.
Wood, E. F.
Zhang, Y.
TI Evaluation of global observations-based evapotranspiration datasets and
IPCC AR4 simulations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID WATER; REANALYSIS; MOISTURE; FLUXNET; SURFACE; SYSTEM
AB Quantification of global land evapotranspiration (ET) has long been associated with large uncertainties due to the lack of reference observations. Several recently developed products now provide the capacity to estimate ET at global scales. These products, partly based on observational data, include satellite-based products, land surface model (LSM) simulations, atmospheric reanalysis output, estimates based on empirical upscaling of eddy-covariance flux measurements, and atmospheric water balance datasets. The LandFlux-EVAL project aims to evaluate and compare these newly developed datasets. Additionally, an evaluation of IPCC AR4 global climate model (GCM) simulations is presented, providing an assessment of their capacity to reproduce flux behavior relative to the observations-based products. Though differently constrained with observations, the analyzed reference datasets display similar large-scale ET patterns. ET from the IPCC AR4 simulations was significantly smaller than that from the other products for India (up to 1 mm/d) and parts of eastern South America, and larger in the western USA, Australia and China. The inter-product variance is lower across the IPCC AR4 simulations than across the reference datasets in several regions, which indicates that uncertainties may be underestimated in the IPCC AR4 models due to shared biases of these simulations. Citation: Mueller, B., et al. (2011), Evaluation of global observations-based evapotranspiration datasets and IPCC AR4 simulations, Geophys. Res. Lett., 38, L06402, doi: 10.1029/2010GL046230.
C1 [Mueller, B.; Seneviratne, S. I.; Corti, T.; Hirschi, M.; Teuling, A. J.] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Jimenez, C.] Observ Paris, LERMA, F-75014 Paris, France.
[Hirschi, M.] MeteoSwiss, Zurich, Switzerland.
[Balsamo, G.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Ciais, P.; Maignan, F.] CEA, CNRS, LSCE, UMR, F-91190 Gif Sur Yvette, France.
[Dirmeyer, P.; Guo, Z.] Ctr Ocean Land Atmosphere Studies, Calverton, MD 20705 USA.
[Fisher, J. B.] CALTECH, Water & Carbon Cycles Grp, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Jung, M.; Reichstein, M.] Max Planck Inst Biochem, D-07745 Jena, Germany.
[McCabe, M. F.] Univ New S Wales, Sch Civil & Environm Engn, Sydney, NSW 2052, Australia.
[Reichle, R.; Rodell, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sheffield, J.; Wood, E. F.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Teuling, A. J.] Wageningen Univ, Hydrol & Quantitat Water Management Grp, Wageningen, Netherlands.
[Wang, K.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Zhang, Y.] CSIRO Land & Water, Canberra, ACT 2601, Australia.
RP Mueller, B (reprint author), Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland.
EM brigitte.mueller@env.ethz.ch; sonia.seneviratne@env.ethz.ch
RI Zhang, Yongqiang/C-5708-2008; Mueller, Brigitte/E-2594-2011; McCabe,
Matthew/G-5194-2011; Seneviratne, Sonia/G-8761-2011; Corti,
Thierry/C-6332-2008; Reichle, Rolf/E-1419-2012; Rodell,
Matthew/E-4946-2012; Wang, Kaicun/F-7813-2012; Reichstein,
Markus/A-7494-2011; Maignan, Fabienne/F-5419-2013; Dirmeyer,
Paul/B-6553-2016
OI Teuling, Adriaan/0000-0003-4302-2835; Fisher,
Joshua/0000-0003-4734-9085; Zhang, Yongqiang/0000-0002-3562-2323;
Mueller, Brigitte/0000-0003-1876-4722; McCabe,
Matthew/0000-0002-1279-5272; Seneviratne, Sonia/0000-0001-9528-2917;
Rodell, Matthew/0000-0003-0106-7437; Wang, Kaicun/0000-0002-7414-5400;
Reichstein, Markus/0000-0001-5736-1112; Dirmeyer,
Paul/0000-0003-3158-1752
NR 22
TC 133
Z9 134
U1 9
U2 50
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 MAR 18
PY 2011
VL 38
AR L06402
DI 10.1029/2010GL046230
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 737XV
UT WOS:000288604700002
ER
PT J
AU Lee, C
Martin, RV
van Donkelaar, A
Lee, H
Dickerson, RR
Hains, JC
Krotkov, N
Richter, A
Vinnikov, K
Schwab, JJ
AF Lee, Chulkyu
Martin, Randall V.
van Donkelaar, Aaron
Lee, Hanlim
Dickerson, Russell R.
Hains, Jennifer C.
Krotkov, Nickolay
Richter, Andreas
Vinnikov, Konstantine
Schwab, James J.
TI SO2 emissions and lifetimes: Estimates from inverse modeling using in
situ and global, space-based (SCIAMACHY and OMI) observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; UNITED-STATES; SULFUR-DIOXIDE;
RADIATIVE-TRANSFER; TROPOSPHERIC SULFATE; 3-DIMENSIONAL MODEL;
PARTICULATE MATTER; NOX EMISSIONS; TRACE GAS; INTEX-B
AB Top-down constraints on global sulfur dioxide (SO2) emissions are inferred through inverse modeling using SO2 column observations from two satellite instruments (SCIAMACHY and OMI). We first evaluated the SO2 column observations with surface SO2 measurements by applying local scaling factors from a global chemical transport model (GEOS-Chem) to SO2 columns retrieved from the satellite instruments. The resulting annual mean surface SO2 mixing ratios for 2006 exhibit a significant spatial correlation (r = 0.86, slope = 0.91 for SCIAMACHY and r = 0.80, slope = 0.79 for OMI) with coincident in situ measurements from monitoring networks throughout the United States and Canada. We evaluate the GEOS-Chem simulation of the SO2 lifetime with that inferred from in situ measurements to verify the applicability of GEOS-Chem for inversion of SO2 columns to emissions. The seasonal mean SO2 lifetime calculated with the GEOS-Chem model over the eastern United States is 13 h in summer and 48 h in winter, compared to lifetimes inferred from in situ measurements of 19 +/- 7 h in summer and 58 +/- 20 h in winter. We apply SO2 columns from SCIAMACHY and OMI to derive a top-down anthropogenic SO2 emission inventory over land by using the local GEOS-Chem relationship between SO2 columns and emissions. There is little seasonal variation in the top-down emissions (< 15%) over most major industrial regions providing some confidence in the method. Our global estimate for annual land surface anthropogenic SO2 emissions (52.4 Tg S yr(-1) from SCIAMACHY and 49.9 Tg S yr(-1) from OMI) closely agrees with the bottom-up emissions (54.6 Tg S yr(-1)) in the GEOS-Chem model and exhibits consistency in global distributions with the bottom-up emissions (r = 0.78 for SCIAMACHY, and r = 0.77 for OMI). However, there are significant regional differences.
C1 [Lee, Chulkyu; Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Lee, Chulkyu] Korea Meteorol Adm, Natl Inst Meteorol Res, Seoul 156720, South Korea.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lee, Hanlim] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
[Dickerson, Russell R.; Vinnikov, Konstantine] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Hains, Jennifer C.] Maryland Dept Environm, Baltimore, MD 21230 USA.
[Krotkov, Nickolay] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Richter, Andreas] Univ Bremen, Inst Environm Phys & Remote Sensing, D-28334 Bremen, Germany.
[Schwab, James J.] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12203 USA.
RP Lee, C (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
RI Richter, Andreas/C-4971-2008; Martin, Randall/C-1205-2014; Chem,
GEOS/C-5595-2014; Krotkov, Nickolay/E-1541-2012; Dickerson,
Russell/F-2857-2010
OI Richter, Andreas/0000-0003-3339-212X; Martin,
Randall/0000-0003-2632-8402; Krotkov, Nickolay/0000-0001-6170-6750;
Dickerson, Russell/0000-0003-0206-3083
FU Health Canada; National Aeronautics and Space Administration (NASA);
Maryland Department of the Environment
FX We thank three anonymous reviewers for helpful comments. The publicly
released Planetary Boundary Layer (PBL) OMI SO2 Level 2 VC
products were obtained from GES Data and Information Service Center
(http://disc.sci.gsfc.nasa.gov/). SO2 slant columns from
SCIAMACHY were obtained from the Institute of Environmental Physics and
Remote Sensing, University of Bremen, Germany
(http://www.iup.uni-bremen.de/). This work was supported by Health
Canada and by the National Aeronautics and Space Administration (NASA).
Aircraft observations were supported by the Maryland Department of the
Environment.
NR 73
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U1 2
U2 39
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 MAR 18
PY 2011
VL 116
AR D06304
DI 10.1029/2010JD014758
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 737YK
UT WOS:000288606300001
ER
PT J
AU Turtle, EP
Perry, JE
Hayes, AG
Lorenz, RD
Barnes, JW
McEwen, AS
West, RA
Del Genio, AD
Barbara, JM
Lunine, JI
Schaller, EL
Ray, TL
Lopes, RMC
Stofan, ER
AF Turtle, E. P.
Perry, J. E.
Hayes, A. G.
Lorenz, R. D.
Barnes, J. W.
McEwen, A. S.
West, R. A.
Del Genio, A. D.
Barbara, J. M.
Lunine, J. I.
Schaller, E. L.
Ray, T. L.
Lopes, R. M. C.
Stofan, E. R.
TI Rapid and Extensive Surface Changes Near Titan's Equator: Evidence of
April Showers
SO SCIENCE
LA English
DT Article
ID CASSINI RADAR OBSERVATIONS; HUYGENS PROBE; LANDING SITE; SOUTH-POLE;
ATMOSPHERE; REFLECTANCE; CONSTRAINTS; CLOUDS; STORMS; RAIN
AB Although there is evidence that liquids have flowed on the surface at Titan's equator in the past, to date, liquids have only been confirmed on the surface at polar latitudes, and the vast expanses of dunes that dominate Titan's equatorial regions require a predominantly arid climate. We report the detection by Cassini's Imaging Science Subsystem of a large low-latitude cloud system early in Titan's northern spring and extensive surface changes (spanning more than 500,000 square kilometers) in the wake of this storm. The changes are most consistent with widespread methane rainfall reaching the surface, which suggests that the dry channels observed at Titan's low latitudes are carved by seasonal precipitation.
C1 [Turtle, E. P.; Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Perry, J. E.; McEwen, A. S.; Schaller, E. L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Hayes, A. G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
[West, R. A.; Ray, T. L.; Lopes, R. M. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Del Genio, A. D.; Barbara, J. M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Lunine, J. I.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Stofan, E. R.] Proxemy Res, Rectortown, VA 20140 USA.
RP Turtle, EP (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM elizabeth.turtle@jhuapl.edu
RI Barnes, Jason/B-1284-2009; Del Genio, Anthony/D-4663-2012; Turtle,
Elizabeth/K-8673-2012; Hayes, Alexander/P-2024-2014; Lorenz,
Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016
OI Barnes, Jason/0000-0002-7755-3530; Del Genio,
Anthony/0000-0001-7450-1359; Turtle, Elizabeth/0000-0003-1423-5751;
Hayes, Alexander/0000-0001-6397-2630; Lorenz, Ralph/0000-0001-8528-4644;
Lopes, Rosaly/0000-0002-7928-3167
FU Cassini-Huygens mission; NASA; ESA; ASI; Hubble Postdoctoral Fellowship
FX We are grateful to all who developed and operate the Cassini-Huygens
mission and to two very helpful anonymous reviewers. Research was
supported by the Cassini-Huygens mission, a cooperative project of NASA,
ESA, and ASI, managed by JPL, a division of the California Institute of
Technology, under a contract with NASA. Supported by a Hubble
Postdoctoral Fellowship (E.L.S.).
NR 34
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U1 2
U2 13
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 MAR 18
PY 2011
VL 331
IS 6023
BP 1414
EP 1417
DI 10.1126/science.1201063
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 736OM
UT WOS:000288504000034
PM 21415347
ER
PT J
AU Tadic, JM
Xu, L
Houk, KN
Moortgat, GK
AF Tadic, Jovan M.
Xu, Lai
Houk, K. N.
Moortgat, Geert K.
TI Photooxidation of n-Octanal in Air: Experimental and Theoretical Study
SO JOURNAL OF ORGANIC CHEMISTRY
LA English
DT Article
ID WAVELENGTH-DEPENDENT PHOTOLYSIS; TROPOSPHERIC CHEMISTRY; FORMALDEHYDE;
KINETICS; PROPIONALDEHYDE; 25-DEGREES-C; TEMPERATURE; ALDEHYDES;
RADICALS; PHASE
AB Dilute mixtures of n-octanal in synthetic air (up to 100 ppm) were photolyzed with fluorescent UV lamps (275-380 nm) at 298 K. The main photooxidation products were 1-hexene, CO, vinyl alcohol, and acetaldehyde. The photolysis rates and the absolute quantum yields were found to be slightly dependent on the total pressure. At 100 Torr, Phi(100) = 0.41 +/- 0.06, whereas at 700 Torr the total quantum yield was Phi(700) = 0.32 +/- 0.02. Two decomposition channels were identified: the radical channel C(7)H(15)CHO -> C(7)H(15) + HCO and the molecular channel C(7)H(15)CHO -> C(6)H(12) + CH(2)=CHOH, having absolute quantum yields of 0.022 and 0.108 at 700 Torr the product CH(2)=CHOH tautomerizes to acetaldehyde. Carbon balance data lower than unities suggest the existence of unidentified decomposition channel(s) which substantially contributes to the photolysis. On the basis of experimental and theoretical evidence, n-octanal photolysis predominantly proceeds to form Norrish type II products as the major ones.
C1 [Tadic, Jovan M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Xu, Lai; Houk, K. N.] Univ Calif Los Angeles, Dept Chem & Biochem, Los Angeles, CA 90095 USA.
[Moortgat, Geert K.] Max Planck Inst Chem, Atmospher Chem Dept, D-55020 Mainz, Germany.
RP Tadic, JM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jotadic@lycos.com
RI Liu, Peng/D-1233-2013; Tadic, Jovan/P-3677-2016
FU NASA, Oak Ridge Associated Universities
FX J.M.T. is supported by the NASA Senior Postdoc Program, Oak Ridge
Associated Universities.
NR 36
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U1 0
U2 7
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0022-3263
J9 J ORG CHEM
JI J. Org. Chem.
PD MAR 18
PY 2011
VL 76
IS 6
BP 1614
EP 1620
DI 10.1021/jo102133m
PG 7
WC Chemistry, Organic
SC Chemistry
GA 731XD
UT WOS:000288142800013
PM 21319759
ER
PT J
AU Doughty, DC
Thompson, AM
Schoeberl, MR
Stajner, I
Wargan, K
Hui, WCJ
AF Doughty, D. C.
Thompson, A. M.
Schoeberl, M. R.
Stajner, I.
Wargan, K.
Hui, W. C. J.
TI An intercomparison of tropospheric ozone retrievals derived from two
Aura instruments and measurements in western North America in 2006
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MONITORING INSTRUMENT; SATELLITE; SYSTEM
AB Two recently developed methods for quantifying tropospheric ozone abundances based on Aura data, the Trajectory-enhanced Tropospheric Ozone Residual (TTOR) and an assimilation of Aura data into Goddard Earth Observing System Version 4 (ASM), are compared to ozone measurements from ozonesonde data collected in April-May 2006 during the INTEX Ozonesonde Network Study 2006 (IONS-06) campaign. Both techniques use Ozone Monitoring Instrument (OMI) and Microwave Limb Sounder (MLS) observations. Statistics on column ozone amounts for both products are presented. In general, the assimilation compares better to sonde integrated ozone to 200 hPa (28.6% difference for TTOR versus 2.7% difference for ASM), and both products are biased low. To better characterize the performance of ASM, ozone profiles based on the assimilation are compared to those from ozonesondes. We noted slight negative biases in the lower troposphere, and slight positive biases in the upper troposphere/lower stratosphere (UT/LS), where we observed the greatest variability. Case studies were used to further understand ASM performance. We examine one case from 17 April 2006 at Bratt's Lake, Saskatchewan, where geopotential height gradients appear to be related to an underestimation in the ASM in the UT/LS region. A second case, from 21 April 2006 at Trinidad Head, California, is a situation where the overprediction of ozone in the UT/LS region does not appear to be due to current dynamic conditions but seems to be related to uncertainty in the flow pattern and large differences in MLS observations upstream.
C1 [Doughty, D. C.; Thompson, A. M.; Hui, W. C. J.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Schoeberl, M. R.] Sci & Technol Corp, Hampton, VA 23666 USA.
[Stajner, I.] Noblis Inc, Falls Church, VA 22042 USA.
[Wargan, K.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Wargan, K.] Sci Applicat Int Corp, Beltsville, MD USA.
[Hui, W. C. J.] Trinity Consultants, Dallas, TX 75251 USA.
RP Doughty, DC (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
EM dcd167@psu.edu; amt16@psu.edu; mark.schoeberl@mac.com;
Ivanka.Stajner@noblis.org; krzysztof.wargan-1@nasa.gov;
jhui@trinityconsultants.com
RI Stajner, Ivanka/B-5228-2009; Thompson, Anne /C-3649-2014;
OI Stajner, Ivanka/0000-0001-6103-3939; Thompson, Anne
/0000-0002-7829-0920; Wargan, Krzysztof/0000-0002-3795-2983
FU NASA
FX This work, based on the Masters Theses of D. C. Doughty and W. C. J.
Hui, was sponsored by NASA's Aura Validation (M. J. Kurylo/K. W. Jucks)
and Tropospheric Chemistry (B. G. Doddridge/J. H. Crawford/J. A.
Al-Saadi) programs through grants. We are grateful to S. J. Oltmans, D.
W. Tarasick, and J. C. Witte for the IONS ozonesonde data and to S. K.
Miller for the GEOS meteorological data.
NR 30
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U1 0
U2 2
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 MAR 17
PY 2011
VL 116
AR D06303
DI 10.1029/2010JD014703
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 737YG
UT WOS:000288605900002
ER
PT J
AU Hodges, RR
AF Hodges, R. R.
TI Resolution of the lunar hydrogen enigma
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ATMOSPHERE; EXOSPHERE; SURFACE; HELIUM; MODEL
AB The recent discovery, by instruments on the IBEX and Chandrayaan-1 spacecraft, of significant fluxes of energetic hydrogen atoms escaping from the moon suggests that there are flaws in the common wisdom regarding the interaction of solar wind with lunar regolith that have prevailed in attempts to explain the failure of the Apollo 17 far-ultraviolet spectrometer to detect neutral H in the lunar exosphere. A new theory for the interaction of solar wind with the lunar regolith surface is tested by comparing simulated spectra of reflected energetic neutral hydrogen and protons with analogous neutral spectra from Chandrayaan-1 and proton data from the Kaguya mission. Overall, the theory indicates that roughly 1% of solar wind protons incident on the lunar regolith surface exit as energetic protons, and about 98.5% exit as neutral H with super-escape speeds. The remaining 0.5%, which exit as neutral H atoms with sub-escape speeds, form a tenuous exosphere that is compatible with the levels of Lyman-alpha allowed by Apollo 17 observations. Citation: Hodges, R. R. (2011), Resolution of the lunar hydrogen enigma, Geophys. Res. Lett., 38, L06201, doi: 10.1029/2011GL046688.
C1 [Hodges, R. R.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Hodges, R. R.] NASA Lunar Sci Inst, NASA, Ames Res Ctr, Moffett Field, CA USA.
RP Hodges, RR (reprint author), POB 4384, Boulder, CO 80443 USA.
EM hodges@lasp.colorado.edu
FU NASA [NNG09EE30P, NNX09AD75G]
FX It is a pleasure to acknowledge helpful comments of P. Feldman, D
McComas, M. Wieser, and two anonymous reviewers. This work was supported
by NASA grants NNG09EE30P and NNX09AD75G.
NR 17
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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 MAR 16
PY 2011
VL 38
AR L06201
DI 10.1029/2011GL046688
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 737XN
UT WOS:000288603900003
ER
PT J
AU Benson, JL
Kass, DM
Kleinbohl, A
AF Benson, Jennifer L.
Kass, David M.
Kleinboehl, Armin
TI Mars' north polar hood as observed by the Mars Climate Sounder
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID WATER-ICE CLOUDS; GENERAL-CIRCULATION MODEL; MARTIAN ATMOSPHERE; DUST
AB We have used observations from the Mars Climate Sounder (MCS) to investigate the north polar hood (NPH) water ice clouds, including the first systematic examination of the vertical and nighttime structure. We show that the NPH clouds are present between L-S = 150 degrees (early autumn) and 30 degrees (late spring) and that the clouds always extend to the pole. The daytime (1500 LMST) and nighttime (0300 LMST) clouds both have one layer that extends in altitude from 10 to 40 km above the surface, and the layer falls from its peak with a constant mixing ratio. We find that the cloud optical depth is controlled by the atmospheric thermal structure. The nighttime optical depth values are often higher than the daytime, sometimes due to tidally driven diurnal temperature differences and other times (i.e., L-S = 240 degrees-330 degrees) a result of low temperatures associated with the polar vortex at night. We conclude that polar hood clouds are primarily controlled by the temperature structure and form at the water condensation level.
C1 [Benson, Jennifer L.; Kass, David M.; Kleinboehl, Armin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Benson, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-237, Pasadena, CA 91109 USA.
EM jennifer.benson@jpl.nasa.gov
FU National Aeronautics and Space Administration; Government sponsorship
FX We would like to thank the MCS instrument operations team. We also wish
to thank James Shirley and Fredric Taylor for their helpful comments on
the manuscript. We are also grateful to Michael Wolff and an anonymous
reviewer for their specific recommendations to improve the manuscript.
Work at the Jet Propulsion Laboratory, California Institute of
Technology, was performed under a contract with the National Aeronautics
and Space Administration. Government sponsorship acknowledged.
NR 28
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U1 2
U2 10
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 MAR 16
PY 2011
VL 116
AR E03008
DI 10.1029/2010JE003693
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 737XM
UT WOS:000288603800001
ER
PT J
AU Stramler, K
Del Genio, AD
Rossow, WB
AF Stramler, Kirstie
Del Genio, Anthony D.
Rossow, William B.
TI Synoptically Driven Arctic Winter States
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SURFACE-ENERGY BUDGET; SEA-ICE; MOISTURE TRANSPORT; CLOUD PROPERTIES;
CLIMATE-CHANGE; WATER-VAPOR; TEMPERATURE; AMPLIFICATION; SHEBA; ISCCP
AB The dense network of the Surface Heat Budget of the Arctic (SHEBA) observations is used to assess relationships between winter surface and atmospheric variables as the SHEBA site came under the influence of cyclonic and anticyclonic atmospheric circulation systems. Two distinct and preferred states of subsurface, surface, atmosphere, and clouds occur during the SHEBA winter, extending from the oceanic mixed layer through the troposphere and preceded by same-sign variations in the stratosphere. These states are apparent in distributions of surface temperature, sensible heat and longwave radiation fluxes, ocean heat conduction, cloud-base height and temperature, and in the atmospheric humidity and temperature structure.
Surface and atmosphere are in radiative-turbulent-conductive near-equilibrium during a warm opaquely cloudy-sky state, which persists up to 10 days and usually occurs during the low surface pressure phase of a baroclinic wave, although occasionally occurs during the high surface pressure phase because of low, scattered clouds. Clouds occurring in this state have near-unity emissivity and the lowest bases in the vicinity of, or below, the temperature inversion peak. A cold radiatively clear-sky state persists up to two weeks, and occurs only in the high surface pressure phase of a baroclinic wave. The radiatively clear state has clouds that are too tenuous when surface based or, irrespective of opacity, located too far aloft to contribute significantly to the surface energy budget. There is a 13-K surface temperature difference between the two states, and atmospheric inversion peak temperatures are linearly related to the surface temperature in both states. The snow-sea ice interface temperature oscillates over the course of the winter season, as it cools during the radiatively clear state and is warmed from atmospheric emission above and ocean heat conduction from below during the opaquely cloudy state.
Analysis of satellite data over the Arctic from 70 degrees-90 degrees N indicates that the radiatively clear and opaquely cloudy states observed at SHEBA may be representative of the entire Arctic basin. The results suggest that model formulation inadequacies should be easier to diagnose if modeled energy transfers are compared with observations using process-based metrics that acknowledge the bimodal nature of the Arctic ocean-ice-snow-atmosphere column, rather than monthly and regionally averaged quantities. Climate change projections of thinner Arctic sea ice and larger advective water vapor influxes into the Arctic could yield different frequencies of occupation of the radiatively clear and opaquely cloudy states and higher wintertime temperatures of SHEBA ocean, ice, snow, atmosphere, and clouds-in particular, a wintertime warming of the snow-sea ice interface temperature.
C1 [Stramler, Kirstie] Columbia Univ, New York, NY USA.
[Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rossow, William B.] CUNY City Coll, New York, NY 10031 USA.
RP Stramler, K (reprint author), 3048 Halcyon Court B, Berkeley, CA 94705 USA.
EM kirstie.stramler@gmail.com
RI Del Genio, Anthony/D-4663-2012; Rossow, William/F-3138-2015
OI Del Genio, Anthony/0000-0001-7450-1359;
FU DOE; NASA [NNXD7AN04G]
FX This research was supported by the DOE Atmospheric System Research
Program and the NASA Modeling and Analysis Program (MAP). William B.
Rossow was supported by NASA MAP Grant NNXD7AN04G. We thank the SHEBA
ASFG members Ed Andreas, Chris Fairall, Peter Guest, and Ola Persson for
the surface temperature and flux data, Taneil Uttal, Matthew Shupe, and
Janet Intrieri for the ETL cloud data, Richard Moritz for the rawinsonde
data, and Don Perovich for the subsurface temperature data. We also
thank Yuanchong Zhang for his guidance on acquiring, reading, and land
masking the ISCCP data. Three reviewers provided constructive comments
that improved the paper.
NR 58
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U1 0
U2 10
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD MAR 15
PY 2011
VL 24
IS 6
BP 1747
EP 1762
DI 10.1175/2010JCLI3817.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 754PT
UT WOS:000289869400012
ER
PT J
AU Su, CH
Lehoczky, SL
AF Su, Ching-Hua
Lehoczky, S. L.
TI Melt growth of high-resistivity CdZnTe crystals by controlling Cd
over-pressures
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE Directional solidification; Semiconducting cadmium compounds
ID SINGLE-CRYSTALS
AB In this study, Cd1-xZnx Te crystals, with x=0.20, were grown unseeded by closed-ampoule vertical directional solidification (Bridgman) technique under controlled Cd over-pressures. CdZnTe crystals of high electrical resistivity have been reproducibly obtained with the In dopant concentration of 4-6 ppm, atomic and a Cd reservoir temperature between 785 and 825 degrees C. A combination of three process modifications have contributed to the accomplishment: (1) homogenizing the ampoules of starting materials under the vacuum environment to minimize contamination, (2) performing growth under controlled Cd over-pressures with the optimal In dopant, and (3) controlling post-growth cooling procedures to maintain uniformity of electrical properties over the crystal. Published by Elsevier B.V.
C1 [Su, Ching-Hua; Lehoczky, S. L.] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Engn Directorate, Huntsville, AL 35812 USA.
RP Su, CH (reprint author), NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Engn Directorate, Huntsville, AL 35812 USA.
EM ching.h.su@nasa.gov
FU Advanced Capabilities Division, Exploration Systems Mission Directorate,
NASA Headquarter
FX The author would like to acknowledge the supports of the Advanced
Capabilities Division, Exploration Systems Mission Directorate, NASA
Headquarter.
NR 10
TC 7
Z9 7
U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0248
EI 1873-5002
J9 J CRYST GROWTH
JI J. Cryst. Growth
PD MAR 15
PY 2011
VL 319
IS 1
BP 4
EP 7
DI 10.1016/j.jcrysgro.2010.11.177
PG 4
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA 747SP
UT WOS:000289340000002
ER
PT J
AU Heinbockel, JH
Slaba, TC
Blattnig, SR
Tripathi, RK
Townsend, LW
Handler, T
Gabriel, TA
Pinsky, LS
Reddell, B
Clowdsley, MS
Singleterry, RC
Norbury, JW
Badavi, FF
Aghara, SK
AF Heinbockel, John H.
Slaba, Tony C.
Blattnig, Steve R.
Tripathi, Ram K.
Townsend, Lawrence W.
Handler, Thomas
Gabriel, Tony A.
Pinsky, Lawrence S.
Reddell, Brandon
Clowdsley, Martha S.
Singleterry, Robert C.
Norbury, John W.
Badavi, Francis F.
Aghara, Sukesh K.
TI Comparison of the transport codes HZETRN, HETC and FLUKA for a solar
particle event
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Space radiation; Transport codes; Solar particle event
ID RADIATION-EXPOSURE; VALIDATION; SPACE
AB The protection of astronauts and instrumentation from galactic cosmic rays and solar particle events is one of the primary constraints associated with mission planning in low earth orbit or deep space. To help satisfy this constraint, several computational tools have been developed to analyze the effectiveness of various shielding materials and structures exposed to space radiation. These tools are now being carefully scrutinized through a systematic effort of verification, validation, and uncertainty quantification. In this benchmark study, the deterministic transport code HZETRN is compared to the Monte Carlo transport codes HETC-HEDS and FLUKA for a 30 g/cm(2) water target protected by a 20 g/cm(2) aluminum shield exposed to a parameterization of the February 1956 solar particle event. Neutron and proton fiuences as well as dose and dose equivalent are compared at various depths in the water target. The regions of agreement and disagreement between the three codes are quantified and discussed, and recommendations for future work are given. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Blattnig, Steve R.; Tripathi, Ram K.; Clowdsley, Martha S.; Singleterry, Robert C.; Norbury, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Heinbockel, John H.; Slaba, Tony C.] Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA.
[Townsend, Lawrence W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
[Handler, Thomas] Univ Tennessee, Dept Phys, Knoxville, TN 37996 USA.
[Gabriel, Tony A.] SID, Knoxville, TN 37922 USA.
[Pinsky, Lawrence S.; Reddell, Brandon] Univ Houston, Dept Phys, Houston, TX 77002 USA.
[Badavi, Francis F.] Christopher Newport Univ, Dept Phys, Newport News, VA 23606 USA.
[Aghara, Sukesh K.] Prairie View A&M Univ, Dept Chem Engn, Prairie View, TX 77446 USA.
RP Norbury, JW (reprint author), NASA, Langley Res Ctr, Mail Stop 188E, Hampton, VA 23681 USA.
EM john.w.norbury@nasa.gov
FU NASA [NNL06AA14A, NNL07AA36C, NNL07AA18C]
FX This work was supported, in part, by NASA Grant NNL06AA14A. The
HETC-HEDS data was obtained under NASA contract NNL07AA36C. The FLUKA
data was obtained under NASA contract NNL07AA18C.
NR 40
TC 13
Z9 14
U1 0
U2 3
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 MAR 15
PY 2011
VL 47
IS 6
BP 1079
EP 1088
DI 10.1016/j.asr.2010.11.012
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 739RN
UT WOS:000288735800017
ER
PT J
AU Heinbockel, JH
Slaba, TC
Tripathi, RK
Blattnig, SR
Norbury, JW
Badavi, FF
Townsend, LW
Handler, T
Gabriel, TA
Pinsky, LS
Reddell, B
Aumann, AR
AF Heinbockel, John H.
Slaba, Tony C.
Tripathi, Ram K.
Blattnig, Steve R.
Norbury, John W.
Badavi, Francis F.
Townsend, Lawrence W.
Handler, Thomas
Gabriel, Tony A.
Pinsky, Lawrence S.
Reddell, Brandon
Aumann, Aric R.
TI Comparison of the transport codes HZETRN, HETC and FLUKA for galactic
cosmic rays
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Space radiation; Transport codes; Galactic cosmic ray
ID RADIATION-EXPOSURE; AIRCRAFT CREW; VALIDATION; SPACE
AB The HZETRN deterministic radiation code is one of several tools developed to analyze the effects of harmful galactic cosmic rays (GCR) and solar particle events on mission planning and shielding for astronauts and instrumentation. This paper is a comparison study involving the two Monte Carlo transport codes, HETC-HEDS and FLUKA and the deterministic transport code, HZETRN. Each code is used to transport an ion from the 1977 solar minimum GCR spectrum impinging upon a 20 g/cm(2) aluminum slab followed by a 30 g/cm(2) water slab. This research is part of a systematic effort of verification and validation to quantify the accuracy of HZETRN and determine areas where it can be improved. Comparisons of dose and dose equivalent values at various depths in the water slab are presented in this report. This is followed by a comparison of the proton and forward, backward and total neutron flux at various depths in the water slab. Comparisons of the secondary light ion (2)H, (3)H, (3)He and (4)He fluxes are also examined. (C) 2010 Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Tripathi, Ram K.; Blattnig, Steve R.; Norbury, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Heinbockel, John H.; Slaba, Tony C.] Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA.
[Badavi, Francis F.] Christopher Newport Univ, Newport News, VA 23606 USA.
[Townsend, Lawrence W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
[Handler, Thomas] Univ Tennessee, Dept Phys, Knoxville, TN 37996 USA.
[Gabriel, Tony A.] SID, Knoxville, TN 37922 USA.
[Pinsky, Lawrence S.; Reddell, Brandon] Univ Houston, Dept Phys, Houston, TX 77002 USA.
[Aumann, Aric R.] Analyt Serv & Mat Inc, Hampton, VA 23666 USA.
RP Norbury, JW (reprint author), NASA, Langley Res Ctr, Mail Stop 188E, Hampton, VA 23681 USA.
EM john.w.norbury@nasa.gov
FU NASA [NNL06AA14A, NNL07AA36C, NNL07AA18C]
FX This work was supported, in part, by NASA grant NNL06AA14A. The
HETC-HEDS data was obtained under NASA contract NNL07AA36C. The FLUKA
data was obtained under NASA contract NNL07AA18C. We are very grateful
to the referees and Dr. Alfredo Ferrari for comments leading to
significant improvements in the manuscript.
NR 34
TC 14
Z9 15
U1 0
U2 4
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD MAR 15
PY 2011
VL 47
IS 6
BP 1089
EP 1105
DI 10.1016/j.asr.2010.11.013
PG 17
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 739RN
UT WOS:000288735800018
ER
PT J
AU Vogel, B
Pan, LL
Konopka, P
Gunther, G
Muller, R
Hall, W
Campos, T
Pollack, I
Weinheimer, A
Wei, J
Atlas, EL
Bowman, KP
AF Vogel, B.
Pan, L. L.
Konopka, P.
Guenther, G.
Mueller, R.
Hall, W.
Campos, T.
Pollack, I.
Weinheimer, A.
Wei, J.
Atlas, E. L.
Bowman, K. P.
TI Transport pathways and signatures of mixing in the extratropical
tropopause region derived from Lagrangian model simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID STRATOSPHERE-TROPOSPHERE EXCHANGE; IN-SITU MEASUREMENTS; LOWERMOST
STRATOSPHERE; WATER-VAPOR; MASS-EXCHANGE; NORTHERN-HEMISPHERE; ANNUAL
CYCLE; OZONE; CIRCULATION; AIR
AB Model simulations with the Chemical Lagrangian Model of the Stratosphere (CLaMS) driven by wind fields of the National Center for Environmental Prediction (NCEP) were performed in the midlatitude tropopause region in April 2008 to study two research flights conducted during the START08 campaign. One flight targeted a deep tropospheric intrusion and another flight targeted a deep stratospheric intrusion event, both of them in the vicinity of the subtropical and polar jet. Air masses with strong signatures of mixing between stratospheric and tropospheric air masses were identified from measured CO-O-3 correlations, and the characteristics were reproduced by CLaMS model simulations. CLaMS simulations in turn complement the observations and provide a broader view of the mixed region in physical space. Using artificial tracers of air mass origin within CLaMS yields unique information about the transport pathways and their contribution to the composition in the mixed region from different transport origins. Three different regions are examined to categorize dominant transport processes: (1) on the cyclonic side of the polar jet within tropopause folds where air from the lowermost stratosphere and the cyclonic side of the jet is transported downward into the troposphere, (2) on the anticyclonic side of the polar jet around the 2 PVU surface air masses, where signatures of mixing between the troposphere and lowermost stratosphere were found with large contributions of air masses from low latitudes, and (3) in the lower stratosphere associated with a deep tropospheric intrusion originating in the tropical tropopause layer (TTL). Moreover, the time scale of transport from the TTL into the lowermost stratosphere is in the range of weeks whereas the stratospheric intrusions occur on a time scale of days.
C1 [Vogel, B.; Konopka, P.; Guenther, G.; Mueller, R.] Forschungszentrum Julich, Inst Energy & Climate Res Stratosphere, D-52425 Julich, Germany.
[Pan, L. L.; Hall, W.; Campos, T.; Pollack, I.; Weinheimer, A.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Pollack, I.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Wei, J.] NOAA, Ctr Satellite Applicat & Res, NESDIS, Camp Springs, MD USA.
[Wei, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Atlas, E. L.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine & Atmospher Chem, Miami, FL 33149 USA.
[Bowman, K. P.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
RP Vogel, B (reprint author), Forschungszentrum Julich, Inst Energy & Climate Res Stratosphere, D-52425 Julich, Germany.
EM b.vogel@fz-juelich.de; liwen@ucar.edu; p.konopka@fz-juelich.de;
G.Guenther@fz-juelich.de; ro.mueller@fz-juelich.de; hallb@ucar.edu;
campos@ucar.edu; ilana.pollack@noaa.gov; wein@ucar.edu;
jennifer.c.wei@nasa.gov; eatlas@rsmas.miami.edu; k-bowman@tamu.edu
RI Atlas, Elliot/J-8171-2015; Bowman, Kenneth/A-1345-2012; Pollack,
Ilana/F-9875-2012; Guenther, Gebhard/K-7583-2012; Muller,
Rolf/A-6669-2013; Konopka, Paul/A-7329-2013; Vogel, Barbel/A-9988-2013;
Pan, Laura/A-9296-2008
OI Bowman, Kenneth/0000-0002-2667-8632; Guenther,
Gebhard/0000-0003-4111-6221; Muller, Rolf/0000-0002-5024-9977; Pan,
Laura/0000-0001-7377-2114
FU National Science Foundation (NSF); NFS; NCAR; German Science Foundation
(Deutsche Forschungsgemeinschaft, DFG) [552102]
FX The authors thank three anonymous reviewers for their very helpful
reviews. The START08 experiment is sponsored by the National Science
Foundation (NSF). The authors gratefully acknowledge the instrument
team, cosponsored by NFS and NCAR, and the NCAR Research Aviation
Facility staff for running the flight operation. The work by B. Vogel
was partly funded by the German Science Foundation (Deutsche
Forschungsgemeinschaft, DFG) under contract 552102.
NR 70
TC 22
Z9 23
U1 1
U2 18
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 MAR 15
PY 2011
VL 116
AR D05306
DI 10.1029/2010JD014876
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 737XR
UT WOS:000288604300003
ER
PT J
AU Maloney, P
DeVor, R
Novaes-Card, S
Saitta, E
Quinn, J
Clausen, CA
Geiger, CL
AF Maloney, Phillip
DeVor, Robert
Novaes-Card, Simone
Saitta, Erin
Quinn, Jacqueline
Clausen, Christian A.
Geiger, Cherie L.
TI Dechlorination of polychlorinated biphenyls using magnesium and
acidified alcohols
SO JOURNAL OF HAZARDOUS MATERIALS
LA English
DT Article
DE Polychlorinated biphenyl; Dechlorination; Magnesium; Acetic acid;
Ethanol
ID MAGNESIUM/PALLADIUM BIMETALLIC PARTICLES; DIBENZO-P-DIOXINS; SYSTEMS;
DEGRADATION; SURFACE; PD/FE; MG/PD; PCBS
AB Polychlorinated biphenyls (PCBs) were widely used in industry until their regulation in the 1970s. However, due to their inherent stability, they are still a widespread environmental contaminant. A novel method of degradation of PCBs (via hydrodehalogenation) has been observed using magnesium powder, a carboxylic acid, and alcohol solvents and is described in this paper. The rates of degradation were determined while varying the type of acid (formic, acetic, propionic, butyric, valeric, benzoic, ascorbic, and phosphoric), the amount of magnesium from 0.05 to 0.25g, the amount of acetic acid from 0.5 to 50 mu L and the concentration of PCB-151 from 0.1 to 50 mu g/mL, as well as the alcohol solvent (methanol, ethanol, propanol, butanol, octanol, and decanol). The results of these studies indicate that the most rapid PCB dechlorination is achieved using a matrix consisting of at least 0.02 g Mg/mL ethanol, and 10 mu L acetic acid/mL ethanol in which case 50 ng/mu L of PCB-151 is dechlorinated in approximately 40 min. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Geiger, Cherie L.] Univ Cent Florida, Dept Chem, Orlando, FL 32816 USA.
[DeVor, Robert] ASRC Aerosp, Kennedy Space Ctr, FL 32815 USA.
[Quinn, Jacqueline] NASA, Kennedy Space Ctr, FL 32815 USA.
RP Geiger, CL (reprint author), Univ Cent Florida, Dept Chem, 4000 Cent Florida Blvd,Chem Bldg CH 117, Orlando, FL 32816 USA.
EM cgeiger@mail.ucf.edu
OI Novaes-Card, Simone/0000-0002-6239-6149
NR 24
TC 14
Z9 14
U1 0
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3894
J9 J HAZARD MATER
JI J. Hazard. Mater.
PD MAR 15
PY 2011
VL 187
IS 1-3
BP 235
EP 240
DI 10.1016/j.jhazmat.2011.01.006
PG 6
WC Engineering, Environmental; Engineering, Civil; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 738HL
UT WOS:000288630800027
PM 21296492
ER
PT J
AU Ramasamy, S
Tewari, SN
Lee, KN
Bhatt, RT
Fox, DS
AF Ramasamy, Sivakumar
Tewari, Surendra N.
Lee, Kang N.
Bhatt, Ramakrishna T.
Fox, Dennis S.
TI Mullite-gadolinium silicate environmental barrier coatings for melt
infiltrated SiC/SiC composites
SO SURFACE & COATINGS TECHNOLOGY
LA English
DT Article
DE Fiber reinforced composites; Environmental barrier coatings; Sintering;
Oxidation; Thermal cycling; Electron microscopy
ID SIO2 SCALE VOLATILITY; WATER-VAPOR-PRESSURE; SI3N4 CERAMICS; OXIDATION;
TEMPERATURE; RECESSION; CARBIDE
AB Slurry based mullite/gadolinium silicate (Gd(2)SiO(5)) environmental barrier coatings (EBCs) were developed for melt infiltrated (MI) SiC/SiC composites. The coating chemically adhered well on the substrates. Thermal cycling of uncoated MI-SiC/SiC composites conducted between 1350 degrees C and 90 degrees C (one hour hot and 15 min cold) in a 96.5% H(2)O-3.5% O(2) environment caused severe oxidation damage after 100 cycles resulting in the formation of dense silica layer of about 25 mu m maximum thickness. Mullite/Gd(2)SiO(5) EBCs provided excellent protection to MI-SiC/SiC against moisture damage with significantly less oxidation of the substrate: only about a 2 mu m thick oxide layer formed even after 400 similar thermal cycles. The hair-line cracks formed at the coating/substrate interface after 400 cycles causing partial coating de-lamination. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Ramasamy, Sivakumar; Tewari, Surendra N.] Cleveland State Univ, Cleveland, OH 44115 USA.
[Lee, Kang N.] Rolls Royce Corp, Indianapolis, IN USA.
[Bhatt, Ramakrishna T.; Fox, Dennis S.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Ramasamy, S (reprint author), Cleveland State Univ, 2121 Euclid Ave, Cleveland, OH 44115 USA.
EM s.ramasamy1@csuohio.edu
RI Ramasamy, Sivakumar/B-7514-2012
NR 19
TC 10
Z9 12
U1 2
U2 26
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0257-8972
J9 SURF COAT TECH
JI Surf. Coat. Technol.
PD MAR 15
PY 2011
VL 205
IS 12
BP 3578
EP 3581
DI 10.1016/j.surfcoat.2010.12.031
PG 4
WC Materials Science, Coatings & Films; Physics, Applied
SC Materials Science; Physics
GA 737LZ
UT WOS:000288571600004
ER
PT J
AU D'Arrigo, R
Seager, R
Smerdon, JE
LeGrande, AN
Cook, ER
AF D'Arrigo, Rosanne
Seager, Richard
Smerdon, Jason E.
LeGrande, Allegra N.
Cook, Edward R.
TI The anomalous winter of 1783-1784: Was the Laki eruption or an analog of
the 2009-2010 winter to blame?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID NORTH-ATLANTIC; RECONSTRUCTION; EUROPE; INDEX
AB The multi-stage eruption of the Icelandic volcano Laki beginning in June, 1783 is speculated to have caused unusual dry fog and heat in western Europe and cold in North America during the 1783 summer, and record cold and snow the subsequent winter across the circum-North Atlantic. Despite the many indisputable impacts of the Laki eruption, however, its effect on climate, particularly during the 1783-1784 winter, may be the most poorly constrained. Here we test an alternative explanation for the unusual conditions during this time: that they were caused primarily by a combined negative phase of the North Atlantic Oscillation (NAO) and an El Nino-Southern Oscillation (ENSO) warm event. A similar combination of NAO-ENSO phases was identified as the cause of record cold and snowy conditions during the 2009-2010 winter in Europe and eastern North America. 600-year tree-ring reconstructions of NAO and ENSO indices reveal values in the 1783-1784 winter second only to their combined severity in 2009-2010. Data sources and model simulations support our hypothesis that a combined, negative NAO-ENSO warm phase was the dominant cause of the anomalous winter of 1783-1784, and that these events likely resulted from natural variability unconnected to Laki. Citation: D'Arrigo, R., R. Seager, J. E. Smerdon, A. N. LeGrande, and E. R. Cook (2011), The anomalous winter of 1783-1784: Was the Laki eruption or an analog of the 2009-2010 winter to blame?, Geophys. Res. Lett., 38, L05706, doi: 10.1029/2011GL046696.
C1 [D'Arrigo, Rosanne; Seager, Richard; Smerdon, Jason E.; Cook, Edward R.] Columbia Univ, Earth Inst, Lamont Doherty Earth Observ, Palisades, NY 10694 USA.
[LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP D'Arrigo, R (reprint author), Columbia Univ, Earth Inst, Lamont Doherty Earth Observ, 61 Rte 9W, Palisades, NY 10694 USA.
EM rdd@ldeo.columbia.edu
RI Smerdon, Jason/F-9952-2011; LeGrande, Allegra/D-8920-2012
OI LeGrande, Allegra/0000-0002-5295-0062
FU NOAA/NSF; NOAA [NA10OAR4310137]; NASA; ANL [NOAA-C2D2]
FX RD and EC received past NOAA/NSF funding for Atlantic studies. RS and JS
were funded by NOAA NA10OAR4310137. AL received funds from NASA and ANL
NOAA-C2D2. We thank J. Luterbacher, L. Oman and J. Li for assistance.
LDEO 7441. We thank NASA/GISS for institutional support.
NR 29
TC 14
Z9 14
U1 1
U2 15
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 MAR 15
PY 2011
VL 38
AR L05706
DI 10.1029/2011GL046696
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 737XL
UT WOS:000288603700002
ER
PT J
AU Jones, SL
Lessard, MR
Rychert, K
Spanswick, E
Donovan, E
AF Jones, S. L.
Lessard, M. R.
Rychert, K.
Spanswick, E.
Donovan, E.
TI Large-scale aspects and temporal evolution of pulsating aurora
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PITCH-ANGLE DIFFUSION; MORNINGSIDE AURORAE; FAST SATELLITE; LOSS CONE;
MORPHOLOGY; GENERATION; ELECTRONS; SUBSTORM; REGION; SYOWA
AB Pulsating aurora is a common phenomenon generally believed to occur mainly in the aftermath of a substorm, where dim long-period pulsating patches appear. The study determines the temporal and spatial evolution of pulsating events using two THEMIS all-sky imager stations, at Gillam (66.18 magnetic latitude, 332.78 magnetic longitude, magnetic midnight at 0634 UT) and Fort Smith, (67.38 magnetic latitude, 306.64 magnetic longitude, magnetic midnight at 0806 UT) along roughly the same invariant latitude. Parameters have been calculated from a database of 74 pulsating aurora events from 119 days of good optical data within the period from September 2007 through March 2008 as identified with the Gillam camera. It is shown that the source region of pulsating aurora drifts or expands eastward, away from magnetic midnight, for premidnight onsets and that the spatial evolution is more complicated for postmidnight onsets, which has implications for the source mechanism. The most probable duration of a pulsating aurora event is roughly 1.5 h, while the distribution of possible event durations includes many long (several hours) events. This may suggest that pulsating aurora is not strictly a substorm recovery phase phenomenon but rather a persistent, long-lived phenomenon that may be temporarily disrupted by auroral substorms. Observations from the Gillam station show that in fact, pulsating aurora is quite common with the occurrence rate increasing to around 60% for morning hours, with 69% of pulsating aurora onsets occurring after substorm breakup.
C1 [Jones, S. L.; Lessard, M. R.; Rychert, K.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Spanswick, E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Donovan, E.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
RP Jones, SL (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Code 674, Greenbelt, MD 20771 USA.
EM sarah.l.jones@nasa.gov
RI Jones, Sarah/D-5293-2012; Rychert, Kevin/D-1836-2013;
OI Jones, Sarah/0000-0002-3816-4954; Donovan, Eric/0000-0002-8557-4155
FU NASA [NNX08AT38H]
FX Research at the University of New Hampshire was supported by NASA grant
NNX08AT38H.
NR 36
TC 16
Z9 16
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 MAR 15
PY 2011
VL 116
AR A03214
DI 10.1029/2010JA015840
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737YC
UT WOS:000288605400001
ER
PT J
AU Furst, JU
Strekalov, DV
Elser, D
Aiello, A
Andersen, UL
Marquardt, C
Leuchs, G
AF Fuerst, J. U.
Strekalov, D. V.
Elser, D.
Aiello, A.
Andersen, U. L.
Marquardt, Ch
Leuchs, G.
TI Quantum Light from a Whispering-Gallery-Mode Disk Resonator
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID OPTICAL PARAMETRIC OSCILLATOR; SINGLE-BEAM NOISE; TWIN BEAMS;
NONDEGENERATE; GENERATION; REDUCTION; PHASE
AB Optical parametric down-conversion has proven to be a valuable source of nonclassical light. The process is inherently able to produce twin-beam correlations along with individual intensity squeezing of either parametric beam, when pumped far above threshold. Here, we present for the first time the direct observation of intensity squeezing of -1.2 dB of each of the individual parametric beams in parametric down-conversion by use of a high quality whispering-gallery-mode disk resonator. In addition, we observed twin-beam quantum correlations of -2.7 dB with this cavity. Such resonators feature strong optical confinement and offer tunable coupling to an external optical field. This work exemplifies the potential of crystalline whispering-gallery-mode resonators for the generation of quantum light. The simplicity of this device makes the application of quantum light in various fields highly feasible.
C1 [Fuerst, J. U.; Strekalov, D. V.; Elser, D.; Aiello, A.; Andersen, U. L.; Marquardt, Ch; Leuchs, G.] Max Planck Inst Sci Light, Erlangen, Germany.
[Fuerst, J. U.; Elser, D.; Aiello, A.; Marquardt, Ch; Leuchs, G.] Univ Erlangen Nurnberg, Dept Phys, Erlangen, Germany.
[Strekalov, D. V.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Andersen, U. L.] Tech Univ Denmark, Dept Phys, DK-2800 Lyngby, Denmark.
RP Furst, JU (reprint author), Max Planck Inst Sci Light, Erlangen, Germany.
RI Marquardt, Christoph/E-5332-2011; Elser, Dominique/F-2750-2010;
Andersen, Ulrik/A-5965-2011; Aiello, Andrea/A-7518-2012; Leuchs,
Gerd/G-6178-2012;
OI Marquardt, Christoph/0000-0002-5045-513X; Andersen,
Ulrik/0000-0002-1990-7687; Aiello, Andrea/0000-0003-1647-0448; Leuchs,
Gerd/0000-0003-1967-2766; Elser, Dominique/0000-0003-4852-5036
FU EU; Alexander von Humboldt foundation; IMPRS
FX The authors acknowledge funding from the EU project COMPAS. D. V. S. and
A. A. acknowledge funding from the Alexander von Humboldt foundation and
J. U. F. from IMPRS. J. U. F. and Ch. M. thank Alessandro Villar and
Thomas Bauer for helpful discussions.
NR 26
TC 65
Z9 65
U1 3
U2 36
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD MAR 15
PY 2011
VL 106
IS 11
AR 113901
DI 10.1103/PhysRevLett.106.113901
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 735CG
UT WOS:000288390400002
PM 21469862
ER
PT J
AU Wal, RLV
Bryg, VM
Hays, MD
AF Wal, Randy L. Vander
Bryg, Vicky M.
Hays, Michael D.
TI XPS Analysis of Combustion Aerosols for Chemical Composition, Surface
Chemistry, and Carbon Chemical State
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID SOOT PARTICLES; NANOSTRUCTURE; SPECTROSCOPY; NUCLEATION; EMISSIONS;
GROWTH; IMAGES; FINE; ACID; TEM
AB Carbonaceous aerosols can vary in elemental content, surface chemistry, and carbon nanostructure. Each of these properties is related to the details of soot formation. Fuel source, combustion process (affecting formation and growth conditions), and postcombustion exhaust where oxidation occurs all contribute to the physical structure and surface chemistry of soot. Traditionally such physical and chemical parameters have been measured separately by various techniques. Presented here is the unified measurement of these characteristics using X-ray photoelectron spectroscopy (XPS). In the present study, XPS is applied to combustion soot collected from a diesel engine (running biodiesel and pump-grade fuels); jet engine; and institutional, plant, and residential oil-fired boilers. Elemental composition is mapped by a survey scan over a broad energy range. Surface chemistry and carbon nanostructure are quantified by deconvolution of high-resolution scans over the C1s region. This combination of parameters forms a distinct matrix of identifiers for the soots from these sources.
C1 [Wal, Randy L. Vander] Penn State Univ, Dept Energy & Mineral Engn, University Pk, PA 16802 USA.
[Wal, Randy L. Vander] Penn State Univ, EMS Energy Inst, University Pk, PA 16802 USA.
[Bryg, Vicky M.] NASA, USRA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Hays, Michael D.] US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA.
RP Wal, RLV (reprint author), Penn State Univ, Dept Energy & Mineral Engn, University Pk, PA 16802 USA.
EM ruv12@psu.edu
RI Hays, Michael/E-6801-2013
OI Hays, Michael/0000-0002-4029-8660
NR 41
TC 3
Z9 3
U1 0
U2 32
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
EI 1520-6882
J9 ANAL CHEM
JI Anal. Chem.
PD MAR 15
PY 2011
VL 83
IS 6
BP 1924
EP 1930
DI 10.1021/ac102365s
PG 7
WC Chemistry, Analytical
SC Chemistry
GA 732KE
UT WOS:000288182900010
ER
PT J
AU Vinukollu, RK
Wood, EF
Ferguson, CR
Fisher, JB
AF Vinukollu, Raghuveer K.
Wood, Eric F.
Ferguson, Craig R.
Fisher, Joshua B.
TI Global estimates of evapotranspiration for climate studies using
multi-sensor remote sensing data: Evaluation of three process-based
approaches
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Evapotranspiration; Latent heat flux; Surface energy balance; SEBS;
Penman-Monteith Priestley-Taylor; Interception; Canopy evaporation
ID PRIESTLEY-TAYLOR EQUATION; SURFACE-ENERGY BALANCE; VAPOR-PRESSURE
DIFFERENCE; DATA ASSIMILATION SYSTEM; ATMOSPHERE WATER FLUX; TROPICAL
RAIN-FOREST; LEAF-AREA INDEX; SOIL HEAT-FLUX; LAND-SURFACE; INTERCEPTION
LOSS
AB Three process based models are used to estimate terrestrial heat fluxes and evapotranspiration (ET) at the global scale: a single source energy budget model, a Penman-Monteith based approach, and a Priestley-Taylor based approach. All models adjust the surface resistances or provide ecophysiological constraints to account for changing environmental factors. Evaporation (or sublimation) over snow-covered regions is calculated consistently for all models using a modified Penman equation. Instantaneous fluxes of latent heat computed at the time of satellite overpass are linearly scaled to the equivalent daily evapotranspiration using the computed evaporative fraction and the day-time net radiation. A constant fraction (10% of daytime evaporation) is used to account for the night time evaporation. Interception losses are computed using a simple water budget model. We produce daily evapotranspiration and sensible heat flux for the global land surface at 5 km spatial resolution for the period 2003-2006. With the exception of wind and surface pressure, all model inputs and forcings are obtained from satellite remote sensing.
Satellite-based inputs and model outputs were first carefully evaluated at the site scale on a monthly-mean basis, then as a four-year mean against a climatological estimate of ET over 26 major basins, and finally in terms of a latitudinal profile on an annual basis. Intercomparison of the monthly model estimates of latent and sensible heat fluxes with 12 eddy-covariance towers across the U.S. yielded mean correlation of 0.57 and 0.54, respectively. Satellite-based meteorological datasets of 2 m temperature (0.83), humidity (0.70), incident shortwave radiation (0.64), incident longwave radiation (0.67) were found to agree well at the tower scale, while estimates of wind speed correlated poorly (0.17). Comparisons of the four year mean annual ET for 26 global river basins and global latitudinal profiles with a climatologically estimated ET resulted in a Kendall's tau>0.70. The seasonal cycle over the continents is well represented in the How-libeller plots and the suppression of ET during major droughts in Europe, Australia and the Amazon are well picked up. This study provides the first ever moderate resolution estimates of ET on a global scale using only remote sensing based inputs and forcings, and furthermore the first ever multi-model comparison of process-based remote sensing estimates using the same inputs. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Vinukollu, Raghuveer K.; Wood, Eric F.; Ferguson, Craig R.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08540 USA.
[Fisher, Joshua B.] CALTECH, Water & Carbon Cycles Grp, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vinukollu, RK (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08540 USA.
EM rkvinukollu@gmail.com
OI Fisher, Joshua/0000-0003-4734-9085
FU NASA [NNGO4GQ32G, NNX08AN40A, NNX09AK35G]
FX This work was jointly supported by NASA grants NNGO4GQ32G "A Terrestrial
Evaporation Data Product Using MODIS Data"; NNX08AN40A "Developing
Consistent Earth System Data Records for the Global terrestrial Water
Cycle"; and NNX09AK35G "Development and diagnostic analysis of a
multi-decadal global evaporation product". The data for the current
study were obtained from NASA Langley Research Center Atmospheric
Science Data Center, NASA/USGS Land Processes Distributed Active Archive
Center, Goddard Earth Sciences Data and Information Services Center,
Global Precipitation Climatology Center (GPCC), and the Global River
Discharge Center (GRDC). We would like to thank Dr. Justin Sheffield and
the European Center for Medium-Range Weather Forecasts (ECMWF) for the
VIC land surface model and ERA-interim reanalysis datasets respectively.
Lastly, this work would not have been possible without the use of the
TIGRESS high performance computer center at Princeton University, which
is jointly supported by the Princeton Institute for Computational
Science and Engineering and the Princeton University Office of
Information Technology (PU-01T).
NR 152
TC 141
Z9 155
U1 18
U2 130
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 MAR 15
PY 2011
VL 115
IS 3
BP 801
EP 823
DI 10.1016/j.rse.2010.11.006
PG 23
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 717SJ
UT WOS:000287067400001
ER
PT J
AU Wessels, V
Gangopadhyay, AK
Sahu, KK
Hyers, RW
Canepari, SM
Rogers, JR
Kramer, MJ
Goldman, AI
Robinson, D
Lee, JW
Morris, JR
Kelton, KF
AF Wessels, V.
Gangopadhyay, A. K.
Sahu, K. K.
Hyers, R. W.
Canepari, S. M.
Rogers, J. R.
Kramer, M. J.
Goldman, A. I.
Robinson, D.
Lee, J. W.
Morris, J. R.
Kelton, K. F.
TI Rapid chemical and topological ordering in supercooled liquid Cu46Zr54
SO PHYSICAL REVIEW B
LA English
DT Article
ID BULK METALLIC-GLASS; X-RAY-DIFFRACTION; MOLECULAR-DYNAMICS; STRUCTURAL
MODEL; AMORPHOUS-ALLOYS; FORMING ABILITY; BINARY; TRANSITION
AB Evidence for rapid ordering in a supercooled Cu46Zr54 liquid, obtained from high-energy x-ray diffraction in a containerless processing environment, is presented. Relatively sudden changes were observed in the topological and chemical short-range order near 850 degrees C, a temperature that is 75 degrees C below the liquidus temperature and 465 degrees C above the glass transition temperature. A peak in the specific heat was observed with supercooling, with an onset near 850 degrees C (the same temperature as the onset of ordering) and a maximum near 700 degrees C, consistent with the prediction of a molecular-dynamics calculation using embedded atom potentials. The chemical and topological ordering measured here are in agreement with predictions of a rapid development of chemically ordered icosahedral clusters in the supercooled liquid.
C1 [Wessels, V.; Gangopadhyay, A. K.; Sahu, K. K.; Kelton, K. F.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Hyers, R. W.; Canepari, S. M.] Univ Massachusetts, Dept Mech Engn, Amherst, MA 01003 USA.
[Rogers, J. R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Kramer, M. J.; Goldman, A. I.; Robinson, D.] Iowa State Univ, Ames Lab, US DOE, Ames, IA 50011 USA.
[Kramer, M. J.; Goldman, A. I.; Robinson, D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Robinson, D.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Wessels, V.; Sahu, K. K.] ETH, Dept Mat, CH-8046 Zurich, Switzerland.
[Lee, J. W.; Morris, J. R.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA.
RP Wessels, V (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA.
EM victor.wessels@mat.ethz.ch
RI Morris, J/I-4452-2012
OI Morris, J/0000-0002-8464-9047
FU National Science Foundation [DMR-0606065, DMR-0856199]; NASA
[NNX07AK27G, NNX10AU19G]; US Department of Energy (DOE), Basic Energy
Sciences, Office of Science [DE-AC02-06CH11357, DE-AC02-07CH11358]; Oak
Ridge National Laboratory; Republic of Korea, Ministry of Knowledge
Economy [IAN: 16B642601]; US Department of Energy
FX The work at Washington University was partially supported by the
National Science Foundation under Grants No. DMR-0606065 and No.
DMR-0856199 and by NASA under Contracts No. NNX07AK27G and No.
NNX10AU19G. Use of the Advanced Photon Source is supported by the US
Department of Energy (DOE), Basic Energy Sciences, Office of Science,
under Contract No. DE-AC02-06CH11357. The work at Ames Laboratory was
supported by the US DOE, Office of Science, Basic Energy Sciences under
Contract No. DE-AC02-07CH11358. The work of J.R.M. was sponsored by the
Laboratory Directed Research and Development Program of Oak Ridge
National Laboratory, managed by UT-Battelle, , for the US DOE. J.W.L.'s
research was performed at the Oak Ridge National Laboratory, Materials
Science and Technology Division and sponsored by the Republic of Korea,
Ministry of Knowledge Economy, Visiting Scientists Program, under IAN:
16B642601, with the US Department of Energy.
NR 44
TC 44
Z9 45
U1 6
U2 26
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-0121
J9 PHYS REV B
JI Phys. Rev. B
PD MAR 14
PY 2011
VL 83
IS 9
AR 094116
DI 10.1103/PhysRevB.83.094116
PG 9
WC Physics, Condensed Matter
SC Physics
GA 734EX
UT WOS:000288317900004
ER
PT J
AU Komarevskiy, N
Braginsky, L
Shklover, V
Hafner, C
Lawson, J
AF Komarevskiy, Nikolay
Braginsky, Leonid
Shklover, Valery
Hafner, Christian
Lawson, John
TI Fast numerical methods for the design of layered photonic structures
with rough interfaces
SO OPTICS EXPRESS
LA English
DT Article
ID CRYSTAL WAVE-GUIDES; MULTILAYER SYSTEMS; GENETIC ALGORITHMS; SCATTERING;
MIRRORS; OPTIMIZATION; PROPAGATION; FORMULATION; OPTICS; MEDIA
AB A multilayer approach (MA) and modified boundary conditions (MBC) are proposed as fast and efficient numerical methods for the design of 1D photonic structures with rough interfaces. These methods are applicable for the structures, composed of materials with an arbitrary permittivity tensor. MA and MBC are numerically validated on different types of interface roughness and permittivities of the constituent materials. The proposed methods can be combined with the 4x4 scattering matrix method as a field solver and an evolutionary strategy as an optimizer. The resulted optimization procedure is fast, accurate, numerically stable and can be used to design structures for various applications. (C) 2011 Optical Society of America
C1 [Komarevskiy, Nikolay; Braginsky, Leonid; Shklover, Valery; Hafner, Christian] ETH, Swiss Fed Inst Technol, CH-8092 Zurich, Switzerland.
[Lawson, John] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Komarevskiy, N (reprint author), ETH, Swiss Fed Inst Technol, CH-8092 Zurich, Switzerland.
EM n.komarevskiy@ifh.ee.ethz.ch
RI Braginsky, Leonid/B-5278-2008
OI Braginsky, Leonid/0000-0002-2508-8876
NR 22
TC 1
Z9 1
U1 0
U2 6
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 MAR 14
PY 2011
VL 19
IS 6
BP 5489
EP 5499
DI 10.1364/OE.19.005489
PG 11
WC Optics
SC Optics
GA 741NV
UT WOS:000288871300087
PM 21445187
ER
PT J
AU Anderson, JE
Ducey, MJ
Fast, A
Martin, ME
Lepine, L
Smith, ML
Lee, TD
Dubayah, RO
Hofton, MA
Hyde, P
Peterson, BE
Blair, JB
AF Anderson, Jeanne E.
Ducey, Mark J.
Fast, Andrew
Martin, Mary E.
Lepine, Lucie
Smith, Marie-Louise
Lee, Thomas D.
Dubayah, Ralph O.
Hofton, Michelle A.
Hyde, Peter
Peterson, Birgit E.
Blair, J. Bryan
TI Use of waveform lidar and hyperspectral sensors to assess selected
spatial and structural patterns associated with recent and repeat
disturbance and the abundance of sugar maple (Acer saccharum Marsh.) in
a temperate mixed hardwood and conifer forest
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE lidar; hyperspectral; ice storm; tree mortality; stem volume losses;
Acer saccharum
ID SPECTRAL MIXTURE ANALYSIS; NEW-HAMPSHIRE; ICE STORM; CATASTROPHIC WIND;
CANOPY STRUCTURE; LASER ALTIMETER; NEW-ENGLAND; NEW-YORK; VEGETATION;
HURRICANE
AB Waveform lidar imagery was acquired on September 26, 1999 over the Bartlett Experimental Forest (BEF) in New Hampshire (USA) using NASA's Laser Vegetation Imaging Sensor (LVIS). This flight occurred 20 months after an ice storm damaged millions of hectares of forestland in northeastern North America. Lidar measurements of the amplitude and intensity of ground energy returns appeared to readily detect areas of moderate to severe ice storm damage associated with the worst damage. Southern through eastern aspects on side slopes were particularly susceptible to higher levels of damage, in large part overlapping tracts of forest that had suffered the highest levels of wind damage from the 1938 hurricane and containing the highest levels of sugar maple basal area and biomass. The levels of sugar maple abundance were determined through analysis of the 1997 Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) high resolution spectral imagery and inventory of USFS Northern Research Station field plots. We found a relationship between field measurements of stem volume losses and the LVIS metric of mean canopy height (r(2) = 0.66; root mean square errors = 5.7 m(3)/ha, p < 0.0001) in areas that had been subjected to moderate-to-severe ice storm damage, accurately documenting the short-term outcome of a single disturbance event. C (C) 2011 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.3554639]
C1 [Anderson, Jeanne E.; Martin, Mary E.; Lepine, Lucie] Univ New Hampshire, Complex Syst Res Ctr, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Ducey, Mark J.; Lee, Thomas D.] Univ New Hampshire, Dept Nat Resources & Environm, Durham, NH 03824 USA.
[Smith, Marie-Louise] US Forest Serv, USDA, Washington, DC 20250 USA.
[Dubayah, Ralph O.; Hofton, Michelle A.; Hyde, Peter] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Peterson, Birgit E.] USGS Ctr Earth Resources Observat & Sci, Sioux Falls, SD 57198 USA.
[Blair, J. Bryan] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Branch, Greenbelt, MD 20771 USA.
RP Anderson, JE (reprint author), Univ New Hampshire, Complex Syst Res Ctr, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
EM jeanne.anderson@alumni.unh.edu; mark.ducey@unh.edu; afast@ceunh.unh.edu;
mary.martin@unh.edu; lucie.lepine@unh.edu; marielouisesmith@fs.fed.us;
tom.lee@unh.edu; dubayah@umd.edu; mhofton@umd.edu; bpeterson@usgs.gov;
james.b.blair@nasa.gov
RI Khachadourian, Diana/C-8513-2012; Blair, James/D-3881-2013; Ducey,
Mark/K-1101-2016;
OI Lepine, Lucie/0000-0003-1028-2534
FU University of Maryland, College Park; NASA [NGT5-ESSF/03-0000-0026];
National Research Initiative of the USDA Cooperative State Research,
Education and Extension Service [2003-35101-13646]; U.S. Department of
Agriculture, Forest Service Northern Research Station
FX Lidar data were acquired through the LVIS team in the Laser Remote
Sensing Branch at NASA Goddard Space Flight Center with support from the
University of Maryland, College Park. This research was also funded in
part through a NASA Space Grant to the University of New Hampshire, a
Switzer Environmental Fellowship, and an Earth System Science Fellowship
to the first author (NASA NGT5-ESSF/03-0000-0026). This project was also
supported by the National Research Initiative of the USDA Cooperative
State Research, Education and Extension Service, Grant No.
2003-35101-13646 (Efficient Methods of Sampling Coarse Woody Debris) to
Mark J. Ducey. Portions of this research are based upon data generated
in long-term research studies on the Bartlett Experimental Forest,
funded by the U.S. Department of Agriculture, Forest Service Northern
Research Station.
NR 56
TC 3
Z9 3
U1 3
U2 20
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 MAR 11
PY 2011
VL 5
AR 053504
DI 10.1117/1.3554639
PG 18
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 734VH
UT WOS:000288367600002
ER
PT J
AU Ackermann, M
Ajello, M
Asano, K
Axelsson, M
Baldini, L
Ballet, J
Barbiellini, G
Baring, MG
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Bhat, PN
Bissaldi, E
Blandford, RD
Bonamente, E
Borgland, AW
Bouvier, A
Bregeon, J
Brez, A
Briggs, MS
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Carrigan, S
Casandjian, JM
Cecchi, C
Celik, O
Chaplin, V
Charles, E
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Connaughton, V
Conrad, J
Cutini, S
Dermer, CD
De Angelis, A
De Palma, F
Dingus, BL
Silva, EDCE
Drell, PS
Dubois, R
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Frailis, M
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Goldstein, A
Granot, J
Greiner, J
Grenier, IA
Grove, JE
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashi, K
Hayashida, M
Hays, E
Horan, D
Hughes, RE
Itoh, R
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Kippen, RM
Knodlseder, J
Kocevski, D
Kouveliotou, C
Kuss, M
Lande, J
Latronico, L
Lee, SH
Garde, ML
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Makeev, A
Mazziotta, MN
McBreen, S
McEnery, JE
McGlynn, S
Meegan, C
Mehault, J
Meszaros, P
Michelson, PF
Mizuno, T
Monte, C
Monzani, ME
Moretti, E
Morselli, A
Moskalenko, IV
Murgia, S
Nakajima, H
Nakamori, T
Naumann-Godo, M
Nishino, S
Nolan, PL
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paciesas, WS
Paneque, D
Panetta, JH
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Petrosian, V
Piron, F
Porter, TA
Preece, R
Racusin, JL
Raino, S
Rando, R
Rau, A
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Reyes, LC
Ripken, J
Ritz, S
Roth, M
Ryde, F
Sadrozinski, HFW
Sander, A
Scargle, JD
Strickman, MS
Suson, DJ
Tajima, H
Takahashi, H
Tanaka, T
Tanaka, Y
Thayer, JB
Thayer, JG
Tibaldo, L
Tierney, D
Toma, K
Torres, DF
Tosti, G
Tramacere, A
Uchiyama, Y
Uehara, T
Usher, TL
Vandenbroucke, J
van der Horst, AJ
Vasileiou, V
Vilchez, N
Vitale, V
von Kienlin, A
Waite, AP
Wang, P
Wilson-Hodge, C
Winer, BL
Wood, KS
Wu, XF
Yamazaki, R
Yang, Z
Ylinen, T
Ziegler, M
AF Ackermann, M.
Ajello, M.
Asano, K.
Axelsson, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Baring, M. G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Bhat, P. N.
Bissaldi, E.
Blandford, R. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Bregeon, J.
Brez, A.
Briggs, M. S.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Carrigan, S.
Casandjian, J. M.
Cecchi, C.
Celik, O.
Chaplin, V.
Charles, E.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Connaughton, V.
Conrad, J.
Cutini, S.
Dermer, C. D.
De Angelis, A.
De Palma, F.
Dingus, B. L.
Silva, E. Do Couto E.
Drell, P. S.
Dubois, R.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Frailis, M.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Goldstein, A.
Granot, J.
Greiner, J.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashi, K.
Hayashida, M.
Hays, E.
Horan, D.
Hughes, R. E.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kippen, R. M.
Knoedlseder, J.
Kocevski, D.
Kouveliotou, C.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Garde, M. Llena
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Makeev, A.
Mazziotta, M. N.
McBreen, S.
McEnery, J. E.
McGlynn, S.
Meegan, C.
Mehault, J.
Meszaros, P.
Michelson, P. F.
Mizuno, T.
Monte, C.
Monzani, M. E.
Moretti, E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakajima, H.
Nakamori, T.
Naumann-Godo, M.
Nishino, S.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paciesas, W. S.
Paneque, D.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Petrosian, V.
Piron, F.
Porter, T. A.
Preece, R.
Racusin, J. L.
Raino, S.
Rando, R.
Rau, A.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Reyes, L. C.
Ripken, J.
Ritz, S.
Roth, M.
Ryde, F.
Sadrozinski, H. F. -W.
Sander, A.
Scargle, J. D.
Strickman, M. S.
Suson, D. J.
Tajima, H.
Takahashi, H.
Tanaka, T.
Tanaka, Y.
Thayer, J. B.
Thayer, J. G.
Tibaldo, L.
Tierney, D.
Toma, K.
Torres, D. F.
Tosti, G.
Tramacere, A.
Uchiyama, Y.
Uehara, T.
Usher, T. L.
Vandenbroucke, J.
van der Horst, A. J.
Vasileiou, V.
Vilchez, N.
Vitale, V.
von Kienlin, A.
Waite, A. P.
Wang, P.
Wilson-Hodge, C.
Winer, B. L.
Wood, K. S.
Wu, X. F.
Yamazaki, R.
Yang, Z.
Ylinen, T.
Ziegler, M.
TI DETECTION OF A SPECTRAL BREAK IN THE EXTRA HARD COMPONENT OF GRB 090926A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 090926A)
ID GAMMA-RAY BURSTS; LARGE-AREA TELESCOPE; FERMI OBSERVATIONS; LORENTZ
FACTOR; GEV EMISSION; AFTERGLOW; SWIFT; 080916C; IDENTIFICATION;
RADIATION
AB We report on the observation of the bright, long gamma-ray burst, GRB 090926A, by the Gamma-ray Burst Monitor and Large Area Telescope (LAT) instruments on board the Fermi Gamma-ray Space Telescope. GRB 090926A shares several features with other bright LAT bursts. In particular, it clearly shows a short spike in the light curve that is present in all detectors that see the burst, and this in turn suggests that there is a common region of emission across the entire Fermi energy range. In addition, while a separate high-energy power-law component has already been observed in other gamma-ray bursts, here we report for the first time the detection with good significance of a high-energy spectral break (or cutoff) in this power-law component around 1.4 GeV in the time-integrated spectrum. If the spectral break is caused by opacity to electron-positron pair production within the source, then this observation allows us to compute the bulk Lorentz factor for the outflow, rather than a lower limit.
C1 [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Goldstein, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Preece, R.; Razzano, M.; Takahashi, H.; Toma, K.; Uehara, T.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Brez, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Asano, K.] Tokyo Inst Technol, Interact Res Ctr Sci, Meguro, Tokyo 1528551, Japan.
[Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Axelsson, M.] Lund Observ, SE-22100 Lund, Sweden.
[Axelsson, M.; Conrad, J.; Garde, M. Llena; McGlynn, S.; Moretti, E.; Ripken, J.; Ryde, F.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.] Univ Paris 06, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, 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.
[Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Bastieri, D.; Buson, S.; Lubrano, P.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bhat, P. N.; Briggs, M. S.; Chaplin, V.; Connaughton, V.; Goldstein, A.; Guiriec, S.; Paciesas, W. S.; Preece, R.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Bissaldi, E.; Greiner, J.; McBreen, S.; Orlando, E.; Rau, A.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.] 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.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Celik, O.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Hays, E.; McEnery, J. E.; Racusin, J. L.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, O.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Celik, O.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, O.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Razzaque, S.; Strickman, M. S.; Wood, K. S.] Div Space Sci, Naval Res Lab, Washington, DC 20375 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observat & Space Res, Fairfax, VA 22030 USA.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France.
[Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00044 Rome, Italy.
[De Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[De Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Dingus, B. L.; Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Itoh, R.; Katagiri, H.; Mizuno, T.; Nishino, S.; Uehara, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[Granot, J.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Hughes, R. E.; Sander, A.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Bouvier, A.; Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.; Vilchez, N.] Ctr Etud Spatiale Rayonnements, CNRS UPS, F-31028 Toulouse 4, France.
[Kouveliotou, C.; van der Horst, A. J.; Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[McBreen, S.; Tierney, D.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[McGlynn, S.; Moretti, E.; Ryde, F.; Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Meegan, C.] Univ Space Res Assoc NSSTC, Huntsville, AL 35805 USA.
[Meszaros, P.; Toma, K.; Wu, X. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma, I-00133 Rome, Italy.
[Nakajima, H.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ohno, M.; Okumura, A.; Ozaki, M.; Tanaka, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Razzaque, S.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 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.
[Reposeur, T.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.] 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.
[Wu, X. F.] Joint Ctr Particle Nucl Phys & Cosmol J CPNPC, Nanjing 210093, Peoples R China.
[Wu, X. F.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
[Yamazaki, R.] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2525258, Japan.
[Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden.
[Conrad, J.] KA Wallenberg Fdn, Stockholm, Sweden.
[Tibaldo, L.] IDAPP, Knoxville, TN 37930 USA.
[van der Horst, A. J.] NASA, Postdoctoral Program, Washington, DC USA.
RP Bregeon, J (reprint author), Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
EM amg0005@uah.edu; johan.bregeon@pi.infn.it; Rob.Preece@nasa.gov;
hirotaka@hep01.hepl.hiroshima-u.ac.jp; toma@astro.psu.edu;
uehara@hep01.hepl.hiroshima-u.ac.jp
RI Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Racusin,
Judith/D-2935-2012; Harding, Alice/D-3160-2012; Gehrels,
Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012;
Stecker, Floyd/D-3169-2012; lubrano, pasquale/F-7269-2012; Morselli,
Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013;
Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Funk,
Stefan/B-7629-2015; Gargano, Fabio/O-8934-2015; Loparco,
Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Moskalenko,
Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Bissaldi,
Elisabetta/K-7911-2016; Wu, Xuefeng/G-5316-2015; Torres,
Diego/O-9422-2016; Orlando, E/R-5594-2016;
OI lubrano, pasquale/0000-0003-0221-4806; Morselli,
Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer,
Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Gargano,
Fabio/0000-0002-5055-6395; Loparco, Francesco/0000-0002-1173-5673;
Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko,
Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672;
Bissaldi, Elisabetta/0000-0001-9935-8106; Wu,
Xuefeng/0000-0002-6299-1263; Torres, Diego/0000-0002-1522-9065; Dingus,
Brenda/0000-0001-8451-7450; Giordano, Francesco/0000-0002-8651-2394; De
Angelis, Alessandro/0000-0002-3288-2517; Frailis,
Marco/0000-0002-7400-2135; Preece, Robert/0000-0003-1626-7335; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214;
SPINELLI, Paolo/0000-0001-6688-8864; Rando,
Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862;
Omodei, Nicola/0000-0002-5448-7577; 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; Tramacere, Andrea/0000-0002-8186-3793;
Baldini, Luca/0000-0002-9785-7726
FU K. A. Wallenberg Foundation; International Doctorate on Astroparticle
Physics (IDAPP) program; NASA; DOE in the United States; CEA/Irfu and
IN2P3/CNRS in France; ASI; INFN in Italy; MEXT; KEK; JAXA in Japan;
Swedish Research Council; National Space Board in Sweden; INAF in Italy;
CNES in France
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; Partially supported by the
International Doctorate on Astroparticle Physics (IDAPP) program.; We
thank R. Mochkovitch for useful discussions. The Fermi GBM Collaboration
acknowledges support for GBM development, operations, and data analysis
from NASA in the US and BMWi/DLR in Germany. The Fermi LAT Collaboration
acknowledges support from a number of agencies and institutes for both
the development and the operation of the LAT as well as scientific data
analysis. These include NASA and DOE in the United States, CEA/Irfu and
IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in
Japan, and the K. A. Wallenberg Foundation, the Swedish Research
Council, and the National Space Board in Sweden. Additional support from
INAF in Italy and CNES in France for science analysis during the
operations phase is also gratefully acknowledged.
NR 58
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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 MAR 10
PY 2011
VL 729
IS 2
AR 114
DI 10.1088/0004-637X/729/2/114
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700037
ER
PT J
AU Case, GL
Cherry, ML
Wilson-Hodge, CA
Camero-Arranz, A
Rodi, JC
Chaplin, V
Finger, MH
Jenke, P
Beklen, E
Bhat, PN
Briggs, MS
Connaughton, V
Greiner, J
Kippen, RM
Meegan, CA
Paciesas, WS
Preece, R
von Kienlin, A
AF Case, G. L.
Cherry, M. L.
Wilson-Hodge, C. A.
Camero-Arranz, A.
Rodi, J. C.
Chaplin, V.
Finger, M. H.
Jenke, P.
Beklen, E.
Bhat, P. N.
Briggs, M. S.
Connaughton, V.
Greiner, J.
Kippen, R. M.
Meegan, C. A.
Paciesas, W. S.
Preece, R.
von Kienlin, A.
TI FIRST RESULTS FROM FERMI GAMMA-RAY BURST MONITOR EARTH OCCULTATION
MONITORING: OBSERVATIONS OF SOFT GAMMA-RAY SOURCES ABOVE 100 keV
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: galaxies; gamma rays: stars; methods: observational
ID BLACK-HOLE CANDIDATE; CRAB-NEBULA; HARD STATE; MULTIWAVELENGTH
OBSERVATIONS; BATSE OBSERVATIONS; RXTE OBSERVATIONS; GRS 1915+105;
CENTAURUS-A; CYGNUS X-1; GX 339-4
AB The NaI and BGO detectors on the Gamma-ray Burst Monitor (GBM) on Fermi are now being used for long-term monitoring of the hard X-ray/low-energy gamma-ray sky. Using the Earth occultation technique as demonstrated previously by the BATSE instrument on the Compton Gamma-Ray Observatory, GBM can be used to produce multiband light curves and spectra for known sources and transient outbursts in the 8 keV to 1 MeV energy range with its NaI detectors and up to 40 MeV with its BGO detectors. Over 85% of the sky is viewed every orbit, and the precession of the Fermi orbit allows the entire sky to be viewed every similar to 26 days with sensitivity exceeding that of BATSE at energies below similar to 25 keV and above similar to 1.5 MeV. We briefly describe the technique and present preliminary results using the NaI detectors after the first two years of observations at energies above 100 keV. Eight sources are detected with a significance greater than 7 sigma: the Crab, Cyg X-1, SWIFT J1753.5-0127, 1E 1740-29, Cen A, GRS 1915+105, and the transient sources XTE J1752-223 and GX 339-4. Two of the sources, the Crab and Cyg X-1, have also been detected above 300 keV.
C1 [Case, G. L.; Cherry, M. L.; Rodi, J. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Wilson-Hodge, C. A.; Jenke, P.] George C Marshall Space Flight Ctr, Huntsville, AL 35182 USA.
[Camero-Arranz, A.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Chaplin, V.; Bhat, P. N.; Briggs, M. S.; Greiner, J.; Paciesas, W. S.; Preece, R.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Finger, M. H.; Meegan, C. A.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Beklen, E.] Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey.
[Beklen, E.] Suleyman Demirel Univ, Dept Phys, TR-32260 Isparta, Turkey.
[Greiner, J.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Jenke, P.] NASA, Washington, DC USA.
RP Case, GL (reprint author), Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
EM case@phunds.phys.lsu.edu
OI Preece, Robert/0000-0003-1626-7335
FU NASA; NASA/Louisiana Board of Regents [NNX07AT62A]; Spanish Ministerio
de Ciencia e Innovacion through MICINN/Fulbright [2008-0116]
FX This work is supported by the NASA Fermi Guest Investigator program. At
LSU, additional support is provided by NASA/Louisiana Board of Regents
Cooperative Agreement NNX07AT62A. A. C.-A. thanks the Spanish Ministerio
de Ciencia e Innovacion for support through the 2008 postdoctoral
program MICINN/Fulbright under grant 2008-0116.
NR 61
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U1 0
U2 5
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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 MAR 10
PY 2011
VL 729
IS 2
AR 105
DI 10.1088/0004-637X/729/2/105
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700028
ER
PT J
AU Crepp, JR
Pueyo, L
Brenner, D
Oppenheimer, BR
Zimmerman, N
Hinkley, S
Parry, I
King, D
Vasisht, G
Beichman, C
Hillenbrand, L
Dekany, R
Shao, M
Burruss, R
Roberts, LC
Bouchez, A
Roberts, J
Soummer, R
AF Crepp, Justin R.
Pueyo, Laurent
Brenner, Douglas
Oppenheimer, Ben R.
Zimmerman, Neil
Hinkley, Sasha
Parry, Ian
King, David
Vasisht, Gautam
Beichman, Charles
Hillenbrand, Lynne
Dekany, Richard
Shao, Mike
Burruss, Rick
Roberts, Lewis C.
Bouchez, Antonin
Roberts, Jenny
Soummer, Remi
TI SPECKLE SUPPRESSION WITH THE PROJECT 1640 INTEGRAL FIELD SPECTROGRAPH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: adaptive optics; techniques: high angular resolution;
techniques: spectroscopic
ID HR 8799 B; SUBSTELLAR COMPANION; FU-ORIONIS; DEBRIS DISK; GJ 758;
CONTRAST; STAR; SPECTROSCOPY; DISCOVERY; CORONAGRAPH
AB Project 1640 is a high-contrast imaging instrument recently commissioned at the Palomar observatory. A combination of a coronagraph with an integral-field spectrograph (IFS), Project 1640 is designed to detect and characterize extrasolar planets, brown dwarfs, and circumstellar material orbiting nearby stars. In this paper, we present our data processing techniques for improving upon instrument raw sensitivity via the removal of quasistatic speckles. Our approach utilizes the chromatic image diversity provided by the IFS in combination with the locally optimized combination of images algorithm to suppress the intensity of residual contaminating light in close angular proximity to target stars. We describe the Project 1640 speckle suppression pipeline and demonstrate its ability to detect companions with brightness comparable to and below that of initial speckle intensities using on-sky commissioning data. Our preliminary results indicate that suppression factors of at least one order of magnitude are consistently possible, reaching 5 sigma contrast levels of 2.1 x 10(-5) at 1 '' in the H band in 20 minutes of on-source integration time when non-common-path errors are reasonably well calibrated. These results suggest that near-infrared contrast levels of order approximate to 10(-7) at subarcsecond separations will soon be possible for Project 1640 and similarly designed instruments that receive a diffraction-limited beam corrected by adaptive optics systems employing deformable mirrors with high actuator density.
C1 [Crepp, Justin R.; Hinkley, Sasha; Beichman, Charles; Hillenbrand, Lynne; Dekany, Richard; Bouchez, Antonin] CALTECH, Pasadena, CA 91125 USA.
[Pueyo, Laurent; Vasisht, Gautam; Beichman, Charles; Shao, Mike; Burruss, Rick; Roberts, Lewis C.; Roberts, Jenny] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pueyo, Laurent; Soummer, Remi] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Pueyo, Laurent] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Brenner, Douglas; Oppenheimer, Ben R.; Zimmerman, Neil] Amer Museum Nat Hist, New York, NY 10024 USA.
[Zimmerman, Neil] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Parry, Ian; King, David] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Beichman, Charles] NASA Exoplanet Sci Inst, Pasadena, CA 91122 USA.
RP Crepp, JR (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM jcrepp@astro.caltech.edu
OI Zimmerman, Neil/0000-0001-5484-1516
FU National Science Foundation [AST-0520822, AST-0804417, AST-0908484];
Carl Sagan Fellowship Program; National Aeronautics and Space
Administration (NASA)
FX We are grateful to the staff at Palomar Observatory for their support.
Project 1640 is funded by National Science Foundation Grants
AST-0520822, AST-0804417, and AST-0908484. L.P. and S.H. acknowledge
support from the Carl Sagan Fellowship Program. This work was performed
in part under contract with the California Institute of Technology,
funded by the National Aeronautics and Space Administration (NASA),
through the Sagan Fellowship Program. A portion of the research
presented in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contrast with
NASA.
NR 51
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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 MAR 10
PY 2011
VL 729
IS 2
AR 132
DI 10.1088/0004-637X/729/2/132
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700055
ER
PT J
AU Crow, CA
McFadden, LA
Robinson, T
Meadows, VS
Livengood, TA
Hewagama, T
Barry, RK
Deming, LD
Lisse, CM
Wellnitz, D
AF Crow, Carolyn A.
McFadden, L. A.
Robinson, T.
Meadows, V. S.
Livengood, T. A.
Hewagama, T.
Barry, R. K.
Deming, L. D.
Lisse, C. M.
Wellnitz, Dennis
TI VIEWS FROM EPOXI: COLORS IN OUR SOLAR SYSTEM AS AN ANALOG FOR EXTRASOLAR
PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Earth; Moon; planets and satellites: atmospheres; planets and
satellites: individual (Mars); planets and satellites: surfaces;
scattering
ID MULTICOLOR PHOTOELECTRIC PHOTOMETRY; JOVIAN PLANETS; OPTICAL-PROPERTIES;
BRIGHTER PLANETS; SPECTROPHOTOMETRY; ATMOSPHERE; SEARCH; SPECTRUM;
MISSION; TITAN
AB The first visible-light studies of Earth-sized extrasolar planets will employ photometry or low-resolution spectroscopy. This work uses EPOCh medium-band filter photometry between 350 and 950 nm obtained with the Deep Impact (DI) High Resolution Instrument (HRI) of Earth, the Moon, and Mars in addition to previous full-disk observations of the other six solar system planets and Titan to analyze the limitations of using photometric colors to characterize extrasolar planets. We determined that the HRI 350, 550, and 850 nm filters are optimal for distinguishing Earth from the other planets and separating planets to first order based on their atmospheric and surface properties. Detailed conclusions that can be drawn about exoplanet atmospheres simply from a color-color plot are limited due to potentially competing physical processes in the atmosphere. The presence of a Rayleigh scattering atmosphere can be detected by an increase in the 350-550 nm brightness ratio, but the absence of Rayleigh scattering cannot be confirmed due to the existence of atmospheric and surface absorbing species in the UV. Methane and ammonia are the only species responsible for strong absorption in the 850 nm filter in our solar system. The combination of physical processes present on extrasolar planets may differ from those we see locally. Nevertheless, a generation of telescopes capable of collecting such photometric observations can serve a critical role in first-order characterization and constraining the population of Earth-like extrasolar planets.
C1 [Crow, Carolyn A.; Hewagama, T.; Wellnitz, Dennis] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[McFadden, L. A.; Livengood, T. A.; Hewagama, T.; Barry, R. K.; Deming, L. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Robinson, T.; Meadows, V. S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Livengood, T. A.] Natl Ctr Earth & Space Sci Educ, Greenbelt, MD 20771 USA.
[Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Crow, CA (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RI Wellnitz, Dennis/B-4080-2012; Livengood, Timothy/C-8512-2012; Hewagama,
T/C-8488-2012; McFadden, Lucy-Ann/I-4902-2013; Lisse, Carey/B-7772-2016
OI McFadden, Lucy-Ann/0000-0002-0537-9975; Lisse, Carey/0000-0002-9548-1526
NR 61
TC 10
Z9 10
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
VL 729
IS 2
AR 130
DI 10.1088/0004-637X/729/2/130
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700053
ER
PT J
AU Currie, T
Burrows, A
Itoh, Y
Matsumura, S
Fukagawa, M
Apai, D
Madhusudhan, N
Hinz, PM
Rodigas, TJ
Kasper, M
Pyo, TS
Ogino, S
AF Currie, Thayne
Burrows, Adam
Itoh, Yoichi
Matsumura, Soko
Fukagawa, Misato
Apai, Daniel
Madhusudhan, Nikku
Hinz, Philip M.
Rodigas, T. J.
Kasper, Markus
Pyo, T. -S.
Ogino, Satoshi
TI A COMBINED SUBARU/VLT/MMT 1-5 mu m STUDY OF PLANETS ORBITING HR 8799:
IMPLICATIONS FOR ATMOSPHERIC PROPERTIES, MASSES, AND FORMATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; instrumentation: adaptive optics; planetary systems;
stars: individual (HR 8799); techniques: image processing
ID EXTRASOLAR GIANT PLANETS; YOUNG SOLAR ANALOG; BROWN DWARFS;
BETA-PICTORIS; GRAVITATIONAL-INSTABILITY; CHEMICAL-EQUILIBRIUM;
SUBSTELLAR COMPANION; SUPER-EARTHS; DEBRIS DISK; DISCOVERY
AB We present new 1-1.25 mu m (z and J band) Subaru/IRCS and 2 mu m (K band) VLT/NaCo data for HR 8799 and a re-reduction of the 3-5 mu m MMT/Clio data first presented by Hinz et al. Our VLT/NaCo data yield a detection of a fourth planet at a projected separation of similar to 15 AU-"HR 8799e." We also report new, albeit weak detections of HR 8799b at 1.03 mu m and 3.3 mu m. Empirical comparisons to field brown dwarfs show that at least HR 8799b and HR 8799c, and possibly HR 8799d, have near-to-mid-IR colors/magnitudes significantly discrepant from the L/T dwarf sequence. Standard cloud deck atmosphere models appropriate for brown dwarfs provide only (marginally) statistically meaningful fits to HR 8799b and c for physically implausible small radii. Models with thicker cloud layers not present in brown dwarfs reproduce the planets' spectral energy distributions far more accurately and without the need for rescaling the planets' radii. Our preliminary modeling suggests that HR 8799b has log(g) = 4-4.5, T-eff = 900 K, while HR 8799c, d, and (by inference) e have log(g) = 4-4.5, T-eff = 1000-1200 K. Combining results from planet evolution models and new dynamical stability limits implies that the masses of HR 8799b, c, d, and e are 6-7 M-J, 7-10 M-J, 7-10 M-J, and 7-10 M-J. "Patchy" cloud prescriptions may provide even better fits to the data and may lower the estimated surface gravities and masses. Finally, contrary to some recent claims, forming the HR 8799 planets by core accretion is still plausible, although such systems are likely rare.
C1 [Currie, Thayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Burrows, Adam; Madhusudhan, Nikku] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Itoh, Yoichi; Ogino, Satoshi] Kobe Univ, Grad Sch Sci, Kobe, Hyogo 657, Japan.
[Matsumura, Soko] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Fukagawa, Misato] Osaka Univ, Dept Earth & Space Sci, Grad Sch Sci, Osaka, Japan.
[Apai, Daniel] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hinz, Philip M.; Rodigas, T. J.] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ USA.
[Kasper, Markus] European So Observ, D-85748 Garching, Germany.
[Pyo, T. -S.] Natl Astron Observ Japan, Tokyo, Japan.
RP Currie, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
FU NASA; NASA ATP [NNX07AG80G]; HST [HST-GO-12181.04-A]; JPL/Spitzer
Agreements [1417122, 1348668, 1371432]; ESO [084.C-656]
FX We thank the referee, Jonathan Fortney, for a rapid report and
suggestions which greatly improved our manuscript. Roman Rafikov, Scott
Kenyon, and Ed Thommes provided very detailed, highly informative
discussions regarding planet formation by core accretion and planetary
dynamics. We also thank Kaitlin Kratter and Ruth Murray-Clay for
valuable discussions on the formation of wide-separation planets and
brown dwarf companions, and for aid in producing our Figure 15. Stanimir
Metchev and Marshall Perrin provided useful advice during the beginning
stages of this project. Finally, we thank David Lafreniere for numerous
conversations regarding the technical details of the ADI/LOCI reduction
procedures and for supplying us with some subroutines. T.C. is supported
by a NASA Postdoctoral Fellowship. A.B. acknowledges support in part
under NASA ATP grant NNX07AG80G, HST grant HST-GO-12181.04-A, and
JPL/Spitzer Agreements 1417122, 1348668, and 1371432. This work is based
in part on observations made with ESO Telescopes at the Paranal
Observatory under program ID 084.C-656. 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.
NR 78
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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 MAR 10
PY 2011
VL 729
IS 2
AR 128
DI 10.1088/0004-637X/729/2/128
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700051
ER
PT J
AU Hanot, C
Mennesson, B
Martin, S
Liewer, K
Loya, F
Mawet, D
Riaud, P
Absil, O
Serabyn, E
AF Hanot, C.
Mennesson, B.
Martin, S.
Liewer, K.
Loya, F.
Mawet, D.
Riaud, P.
Absil, O.
Serabyn, E.
TI IMPROVING INTERFEROMETRIC NULL DEPTH MEASUREMENTS USING STATISTICAL
DISTRIBUTIONS: THEORY AND FIRST RESULTS WITH THE PALOMAR FIBER NULLER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: high angular resolution; instrumentation:
interferometers; methods: data analysis; methods: statistical
ID BEAM COMBINER; DIAMETERS; LIGHT
AB A new "self-calibrated" statistical analysis method has been developed for the reduction of nulling interferometry data. The idea is to use the statistical distributions of the fluctuating null depth and beam intensities to retrieve the astrophysical null depth (or equivalently the object's visibility) in the presence of fast atmospheric fluctuations. The approach yields an accuracy much better (about an order of magnitude) than is presently possible with standard data reduction methods, because the astrophysical null depth accuracy is no longer limited by the magnitude of the instrumental phase and intensity errors but by uncertainties on their probability distributions. This approach was tested on the sky with the two-aperture fiber nulling instrument mounted on the Palomar Hale telescope. Using our new data analysis approach alone-and no observations of calibrators-we find that error bars on the astrophysical null depth as low as a few 10(-4) can be obtained in the near-infrared, which means that null depths lower than 10(-3) can be reliably measured. This statistical analysis is not specific to our instrument and may be applicable to other interferometers.
C1 [Hanot, C.; Riaud, P.; Absil, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Mennesson, B.; Martin, S.; Liewer, K.; Loya, F.; Mawet, D.; Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hanot, C (reprint author), Univ Liege, Inst Astrophys & Geophys, Allee 6 Aout,17 Bat,B5c, B-4000 Liege, Belgium.
EM hanot@astro.ulg.ac.be
FU National Aeronautics and Space Administration; Fond National de la
Recherche scientifique de Belgique (FNRS); Fonds pour la formation a la
Recherche dans l'Industrie et dans l'Agriculture de Belgique (FRIA);
Communaute Francaise de Belgique-Action de recherche concertee-Academie
Wallonie-Europe; Center for Exoplanet Science
FX This work was carried out at the Jet propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. The data presented in this paper are based on
observations obtained at the Hale Telescope, Palomar Observatory, as
part of a continuing collaboration between Caltech, NASA/JPL, and
Cornell University. We wish to thank the Palomar Observatory staff for
their assistance in mounting the PFN and conducting the observations at
the Hale telescope. The research was supported by the Fond National de
la Recherche scientifique de Belgique (FNRS), by the Fonds pour la
formation a la Recherche dans l'Industrie et dans l'Agriculture de
Belgique (FRIA), and by the Communaute Francaise de Belgique-Action de
recherche concertee-Academie Wallonie-Europe and by the Center for
Exoplanet Science. The authors thank the referee for a careful review
and for giving us relevant comments that helped to significantly improve
the paper.
NR 24
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PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
VL 729
IS 2
AR 110
DI 10.1088/0004-637X/729/2/110
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700033
ER
PT J
AU Hathaway, DH
Rightmire, L
AF Hathaway, David H.
Rightmire, Lisa
TI VARIATIONS IN THE AXISYMMETRIC TRANSPORT OF MAGNETIC ELEMENTS ON THE
SUN: 1996-2010
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: dynamo; Sun: rotation; Sun: surface magnetism
ID SOLAR ROTATION MEASUREMENTS; MICHELSON DOPPLER IMAGER; FLUX TRANSPORT;
TORSIONAL OSCILLATION; MERIDIONAL FLOW; MOUNT-WILSON; CYCLE; FIELD;
FEATURES; PHOTOSPHERE
AB We measure the axisymmetric transport of magnetic flux on the Sun by cross-correlating narrow strips of data from line-of-sight magnetograms obtained at a 96 minute cadence by the MDI instrument on the ESA/NASA SOHO spacecraft and then averaging the flow measurements over each synodic rotation of the Sun. Our measurements indicate that the axisymmetric flows vary systematically over the solar cycle. The differential rotation is weaker at maximum than at minimum. The meridional flow is faster at minimum and slower at maximum. The meridional flow speed on the approach to the Cycle 23/24 minimum was substantially faster than it was at the Cycle 22/23 minimum. The average latitudinal profile is largely a simple sinusoid that extends to the poles and peaks at about 35 degrees latitude. As the cycle progresses, a pattern of inflows toward the sunspot zones develops and moves equatorward in step with the sunspot zones. These inflows are accompanied by the torsional oscillations. This association is consistent with the effects of the Coriolis force acting on the inflows. The equatorward motions associated with these inflows are identified as the source of the decrease in net poleward flow at cycle maxima. We also find polar countercells (equatorward flow at high latitudes) in the south from 1996 to 2000 and in the north from 2002 to 2010. We show that these measurements of the flows are not affected by the nonaxisymmetric diffusive motions produced by supergranulation.
C1 [Hathaway, David H.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Rightmire, Lisa] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM david.hathaway@nasa.gov; lar0009@uah.edu
FU NASA
FX D.H. thanks NASA for its support of this research through a grant from
the Heliophysics Causes and Consequences of the Minimum of Solar Cycle
23/24 Program to NASA Marshall Space Flight Center. L.R. thanks NASA for
its support through an EPSCoR grant to Dr. Gary P. Zank through The
University of Alabama in Huntsville. SOHO is a project of international
cooperation between ESA and NASA.
NR 50
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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 MAR 10
PY 2011
VL 729
IS 2
AR 80
DI 10.1088/0004-637X/729/2/80
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700003
ER
PT J
AU Kim, HJ
Evans, NJ
Dunham, MM
Chen, JH
Lee, JE
Bourke, TL
Huard, TL
Shirley, YL
De Vries, C
AF Kim, Hyo Jeong
Evans, Neal J., II
Dunham, Michael M.
Chen, Jo-Hsin
Lee, Jeong-Eun
Bourke, Tyler L.
Huard, Tracy L.
Shirley, Yancy L.
De Vries, Christopher
TI THE SPITZER C2D SURVEY OF NEARBY DENSE CORES. XI. INFRARED AND
SUBMILLIMETER OBSERVATIONS OF CB130
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: ISM; ISM: individual objects (CB130); stars:
formation; stars: low-mass; submillimeter: ISM
ID MASS STAR-FORMATION; MULTIBAND IMAGING PHOTOMETER; PRE-PROTOSTELLAR
CORES; MOLECULAR CLOUD CORES; YOUNG STELLAR OBJECTS; LOW-LUMINOSITY
OBJECT; 1ST HYDROSTATIC CORE; CLASS-I PROTOSTARS; ARRAY CAMERA IRAC;
SPACE-TELESCOPE
AB We present new observations of the CB130 region composed of three separate cores. Using the Spitzer Space Telescope, we detected a Class 0 and a Class II object in one of these, CB130-1. The observed photometric data from Spitzer and ground-based telescopes are used to establish the physical parameters of the Class 0 object. Spectral energy distribution fitting with a radiative transfer model shows that the luminosity of the Class 0 object is 0.14-0.16 L-circle dot, which is low for a protostellar object. In order to constrain the chemical characteristics of the core having the low-luminosity object, we compare our molecular line observations to models of lines including abundance variations. We tested both ad hoc step function abundance models and a series of self-consistent chemical evolution models. In the chemical evolution models, we consider a continuous accretion model and an episodic accretion model to explore how variable luminosity affects the chemistry. The step function abundance models can match observed lines reasonably well. The best-fitting chemical evolution model requires episodic accretion and the formation of CO2 ice from CO ice during the low-luminosity periods. This process removes C from the gas phase, providing a much improved fit to the observed gas-phase molecular lines and the CO2 ice absorption feature. Based on the chemical model result, the low luminosity of CB130-1 is explained better as a quiescent stage between episodic accretion bursts rather than being at the first hydrostatic core stage.
C1 [Kim, Hyo Jeong; Evans, Neal J., II; Dunham, Michael M.; Chen, Jo-Hsin] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Chen, Jo-Hsin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lee, Jeong-Eun] Sejong Univ, Dept Astron & Space Sci, Astrophys Res Ctr Struct & Evolut Cosmos, Seoul 143747, South Korea.
[Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Huard, Tracy L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[De Vries, Christopher] Calif State Univ Stanislaus, Turlock, CA 95382 USA.
RP Kim, HJ (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn,C1400, Austin, TX 78712 USA.
EM hyojeong@astro.as.utexas.edu
RI Lee , Jeong-Eun/E-2387-2013
FU NASA [1224608, 1288664, 1407, NNX07AJ72G, 1279198, 1288806, 1342425];
NSF [AST-0607793, AST-0708158]; Korea government (MEST) [2009-0062866];
Ministry of Education, Science and Technology [2010-0008704]
FX We thank the Lorentz Center in Leiden for hosting several meetings that
contributed to this paper. Support for this work, part of the Spitzer
Legacy Science Program, was provided by NASA through contracts 1224608
and 1288664 issued by the Jet Propulsion Laboratory, California
Institute of Technology, under NASA contract 1407. Support was also
provided by NASA Origins grant NNX07AJ72G and NSF grant AST-0607793 to
the University of Texas at Austin. This research was also supported by
the National Research Foundation of Korea (NRF) grant funded by the
Korea government (MEST; No. 2009-0062866) and by Basic Science Research
Program through the NRF funded by the Ministry of Education, Science and
Technology (No. 2010-0008704). T.L.B. was partially supported by NASA
through contracts 1279198, 1288806, and 1342425 issued by the Jet
Propulsion Laboratory, California Institute of Technology to the
Smithsonian Astrophysical Observatory, and by the NSF through grant
AST-0708158.
NR 75
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Z9 16
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
VL 729
IS 2
AR 84
DI 10.1088/0004-637X/729/2/84
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700007
ER
PT J
AU Maeda, K
Kataoka, J
Nakamori, T
Stawarz, L
Makiya, R
Totani, T
Cheung, CC
Donato, D
Gehrels, N
Parkinson, PS
Kanai, Y
Kawai, N
Tanaka, Y
Sato, R
Takahashi, T
Takahashi, Y
AF Maeda, K.
Kataoka, J.
Nakamori, T.
Stawarz, L.
Makiya, R.
Totani, T.
Cheung, C. C.
Donato, D.
Gehrels, N.
Parkinson, P. Saz
Kanai, Y.
Kawai, N.
Tanaka, Y.
Sato, R.
Takahashi, T.
Takahashi, Y.
TI UNRAVELING THE NATURE OF UNIDENTIFIED HIGH GALACTIC LATITUDE FERMI/LAT
GAMMA-RAY SOURCES WITH SUZAKU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; gamma rays: general; pulsars: general; radiation
mechanisms: non-thermal; X-rays: general
ID LARGE-AREA TELESCOPE; ALL-SKY SURVEY; RADIO GALAXY; SOURCE 3EG;
SPACE-TELESCOPE; PSR J2021+3651; EGRET SOURCES; SOURCE LIST; EMISSION;
CATALOG
AB Here we report on the results of deep X-ray follow-up observations of four unidentified gamma-ray sources detected by the Fermi/LAT instrument at high Galactic latitudes using the X-ray Imaging Spectrometers on board the Suzaku satellite. All of the studied objects were detected with high significance during the first three months of Fermi/LAT operation and subsequently better localized in the first Fermi/LAT catalog (1FGL). For some of them, possible associations with pulsars and active galaxies have subsequently been discussed, and our observations provide an important contribution to this debate. In particular, a bright X-ray point source has been found within the 95% confidence error circle of 1FGL J1231.1-1410. The X-ray spectrum of the discovered Suzaku counterpart of 1FGL J1231.1-1410 is well fitted by a blackbody with an additional power-law component. This supports the recently claimed identification of this source with a millisecond pulsar PSR J1231-1411. For the remaining three Fermi objects, on the other hand, the X-ray observations performed are less conclusive. In the case of 1FGL J1311.7-3429, two bright X-ray point sources were found within the LAT 95% error circle. Even though the X-ray spectral and variability properties for these sources were robustly assessed, their physical nature and relationship with the gamma-ray source remain uncertain. Similarly, we found several weak X-ray sources in the field of 1FGL J1333.2+5056, one coinciding with the high-redshift blazar CLASS J1333+5057. We argue that the available data are consistent with the physical association between these two objects, although the large positional uncertainty of the gamma-ray source hinders a robust identification. Finally, we have detected an X-ray point source in the vicinity of 1FGL J2017.3+0603. This Fermi object was recently suggested to be associated with a newly discovered millisecond radio pulsar PSR J2017+0603, because of the spatial coincidence and the detection of the gamma-ray pulsations in the light curve of 1FGL J2017.3+0603. Interestingly, we have detected the X-ray counterpart of the high-redshift blazar CLASS J2017+0603, located within the error circle of the gamma-ray source, while we were only able to determine an X-ray flux upper limit at the pulsar position. All in all, our studies indicate that while a significant fraction of unidentified high Galactic latitude gamma-ray sources is related to the pulsar and blazar phenomena, associations with other classes of astrophysical objects are still valid options.
C1 [Maeda, K.; Kataoka, J.; Nakamori, T.; Takahashi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Stawarz, L.; Tanaka, Y.; Sato, R.; Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525510, Japan.
[Stawarz, L.] Jagiellonian Univ, PL-30244 Krakow, Poland.
[Makiya, R.; Totani, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Cheung, C. C.] NRC Res Associate, Div Space Sci, Naval Res Lab, Washington, DC 20375 USA.
[Donato, D.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Parkinson, P. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Kanai, Y.; Kawai, N.] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan.
RP Maeda, K (reprint author), Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, 3-4-1Okubo, Tokyo 1698555, Japan.
EM ko-t.maeda.x-6@ruri.waseda.jp
RI Gehrels, Neil/D-2971-2012; XRAY, SUZAKU/A-1808-2009
FU Polish MNiSW [N-N203-380336]
FX L.S. is grateful for the support from Polish MNiSW through grant
N-N203-380336.
NR 66
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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 MAR 10
PY 2011
VL 729
IS 2
AR 103
DI 10.1088/0004-637X/729/2/103
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700026
ER
PT J
AU Ng, CY
Kaspi, VM
Dib, R
Olausen, SA
Scholz, P
Guver, T
Ozel, F
Gavriil, FP
Woods, PM
AF Ng, C. -Y.
Kaspi, V. M.
Dib, R.
Olausen, S. A.
Scholz, P.
Guever, T.
Oezel, F.
Gavriil, F. P.
Woods, P. M.
TI CHANDRA AND RXTE OBSERVATIONS OF 1E 1547.0-5408: COMPARING THE 2008 AND
2009 OUTBURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (1E 1547.0-5408, PSR J1550-5418, SGR J1550-5418);
stars: neutron; X-rays: bursts
ID X-RAY PULSAR; RESONANT CYCLOTRON SCATTERING; SOFT GAMMA REPEATERS;
SPIN-DOWN; NEUTRON-STARS; MAGNETAR; EMISSION; 1E-1547.0-5408;
1E-1048.1-5937; PERSISTENT
AB We present results from Chandra X-ray Observatory and Rossi X-ray Timing Explorer (RXTE) observations of the magnetar 1E 1547.0-5408 (SGR J1550-5418) following the source's outbursts in 2008 October and 2009 January. During the time span of the Chandra observations, which covers days 4 through 23 and days 2 through 16 after the 2008 and 2009 events, respectively, the source spectral shape remained stable in the Chandra band, while the pulsar's spin-down rate in the same span in 2008 increased by a factor of 2.2 as measured by RXTE. This suggests decoupling between the source's spin-down and radiative changes, hence between the spin-down-inferred magnetic field strength and that inferred spectrally. The lack of spectral variation during flux decay is surprising for models of magnetar outbursts. We also found a strong anti-correlation between the phase-averaged flux and the pulsed fraction in the 2008 and 2009 Chandra data, but not in the pre-2008 measurements. We discuss these results in the context of the magnetar model.
C1 [Ng, C. -Y.; Kaspi, V. M.; Dib, R.; Olausen, S. A.; Scholz, P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Guever, T.; Oezel, F.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Gavriil, F. P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Gavriil, F. P.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
[Woods, P. M.] Corvid Technol, Huntsville, AL 35806 USA.
RP Ng, CY (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
EM ncy@hep.physics.mcgill.ca
RI Guver, Tolga/C-1408-2011; Guver, Tolga/B-1039-2014; Ng, Chi
Yung/A-7639-2013
OI Guver, Tolga/0000-0002-3531-9842; Ng, Chi Yung/0000-0002-5847-2612
FU NSERC; CIFAR; FQRNT via CRAQ
FX We thank A. Archibald, S. Bogdanov, M. Livingstone, and W. Zhu for
useful discussions. C.-Y.N. is a CRAQ postdoctoral fellow. V.M.K. holds
the Lorne Trottier Chair in Astrophysics and Cosmology and a Canada
Research Chair in Observational Astrophysics. This work is supported by
an NSERC Discovery Grant, by CIFAR, and by FQRNT via CRAQ.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
VL 729
IS 2
AR 131
DI 10.1088/0004-637X/729/2/131
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700054
ER
PT J
AU Radeva, YL
Mumma, MJ
Villanueva, GL
A'Hearn, MF
AF Radeva, Yana L.
Mumma, Michael J.
Villanueva, Geronimo L.
A'Hearn, Michael F.
TI A NEWLY DEVELOPED FLUORESCENCE MODEL FOR C2H6 nu(5) AND APPLICATION TO
COMETARY SPECTRA ACQUIRED WITH NIRSPEC AT KECK II
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; comets: individual (C/2004 Q2 Machholz, C/2000 WM1
LINEAR); infrared: general; molecular data; techniques: spectroscopic
ID GIOTTO SPACECRAFT ENCOUNTER; MONTE-CARLO-SIMULATION; ATMOSPHERES
APPLICATION; INFRARED FLUORESCENCE; PARENT VOLATILES; MOLECULES;
EMISSION; ETHANE; IDENTIFICATION; FORMALDEHYDE
AB Accurate rotational temperatures are essential for extracting production rates for parent volatiles in comets. Two strong bands of ethane (nu(7) at 2985.39 cm(-1) and nu(5) at 2895.67 cm(-1)) are seen in infrared cometary spectra, but the Q-branches of nu(7) are not resolved by current instruments and cannot provide an accurate rotational temperature with current models. We developed a fluorescence model for the C2H6 nu(5) band that can be used to derive a rotational temperature. We applied our C2H6 nu(5) model to high-resolution infrared spectra of the comets C/2004 Q2 Machholz and C/2000 WM1 (LINEAR), acquired with the Near-infrared Echelle Spectrograph on the Keck II telescope. We demonstrate agreement among the rotational temperatures derived from C2H6 nu(5) and other species, and between mixing ratios derived from C2H6 nu(5) and C2H6 nu(7). As a symmetric hydrocarbon, C2H6 is observed only in the infrared, and it is now the fifth molecule (along with H2O, HCN, CO, and H2CO) for which we can derive a reliable rotational temperature from cometary infrared spectra.
C1 [Radeva, Yana L.; Mumma, Michael J.; Villanueva, Geronimo L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Radeva, Yana L.; Villanueva, Geronimo L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Radeva, Yana L.; A'Hearn, Michael F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Radeva, YL (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM yana.l.radeva@nasa.gov
RI mumma, michael/I-2764-2013
FU NASA [RTOP 344-32-07, 08-PAST08-0034, 08-PATM08-0031]; Astrobiology
Institute [RTOP 344-53-51]; W.M. Keck Foundation
FX This work was completed as part of Y.L.R.'s Ph.D. dissertation at the
University of Maryland, College Park, and was supported by NASA
(Planetary Astronomy Program (RTOP 344-32-07 to MJM), Astrobiology
Institute (RTOP 344-53-51 to MJM)). G.L.V. acknowledges support from
NASA's Planetary Astronomy Program (08-PAST08-0034) and NASA's Planetary
Atmospheres Program (08-PATM08-0031). The data presented herein were
obtained at the W.M. Keck Observatory, operated as a scientific
partnership among CalTech, UCLA, and NASA. This Observatory was made
possible by the generous financial support of the W.M. Keck Foundation.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
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IS 2
AR 135
DI 10.1088/0004-637X/729/2/135
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700058
ER
PT J
AU Ricca, A
Bauschlicher, CW
Allamandola, LJ
AF Ricca, Alessandra
Bauschlicher, Charles W., Jr.
Allamandola, Louis J.
TI THE INFRARED SPECTROSCOPY OF POLYCYCLIC AROMATIC HYDROCARBONS WITH FIVE-
AND SEVEN-MEMBERED FUSED RING DEFECTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: ISM; ISM: lines and bands; ISM: molecules;
line: identification; methods: numerical; molecular data
ID MU-M; SYMMETRY-BREAKING; LARGE MOLECULES; FAR-IR; PAHS; SPECTRA;
EMISSION; FEATURES; DUST; IDENTIFICATION
AB Polycyclic aromatic hydrocarbon (PAH) growth and destruction are thought to proceed via the occasional incorporation of five-and seven-membered fused ring defects in the hexagonal carbon skeleton. Using density functional theory, this paper investigates the effect such five-and seven-membered fused ring defects have on the infrared spectra of ovalene, circumovalene, and circumcircumovalene. The defects make only small changes to the overall infrared (IR) spectra, both in the mid-IR and in the far-IR, of these species. In addition to small shifts in the positions of the bands between the PAHs with and without defects, the most common effect of the defects is to increase the number of bands. Except for an anion with the Stone-Wales defect, all of the species studied have the C-C stretching band at 6.3 mu m or at longer wavelengths, the position in Classes B and C astronomical PAH spectra. In the case of the Stone-Wales anion, the band falls at 6.20 mu m, suggesting that further study of defects is probably worthwhile, as some PAHs with defects might be important in those sources (Class A) that show a C-C stretching band that falls near 6.2 mu m.
C1 [Ricca, Alessandra] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA.
[Allamandola, Louis J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Ricca, A (reprint author), Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
EM Alessandra.Ricca-1@nasa.gov; Charles.W.Bauschlicher@nasa.gov;
Louis.J.Allamandola@nasa.gov
FU NASA
FX We thank NASA's Astrophysics Theory and Fundamental Physics (ATFP)
(NNX09AD18G) program for its generous support of this work. L.J.A.
acknowledges support from NASA's Astrobiology and Laboratory
Astrophysics Programs.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
VL 729
IS 2
AR 94
DI 10.1088/0004-637X/729/2/94
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700017
ER
PT J
AU Sloan, GC
Hony, S
Smolders, K
Decin, L
Zijlstra, AA
Feast, MW
van Wyk, F
van Loon, JT
Groenewegen, MAT
Sahai, R
AF Sloan, G. C.
Hony, S.
Smolders, K.
Decin, L.
Zijlstra, A. A.
Feast, M. W.
van Wyk, F.
van Loon, J. Th.
Groenewegen, M. A. T.
Sahai, R.
TI THE IDENTIFICATION OF PROBABLE SiS EMISSION AT 13-14 mu m IN SPECTRA OF
GALACTIC S STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars; stars: AGB and post-AGB; stars:
mass-loss
ID ALL-SKY SURVEY; STANDARD CALIBRATION STARS; SPITZER-SPACE-TELESCOPE;
RICH CIRCUMSTELLAR DUST; GIANT BRANCH STARS; ISO-SWS SPECTRA;
OPTICAL-PROPERTIES; INFRARED-SPECTRA; ALUMINUM-OXIDE; AGB STARS
AB A sample of 90 Galactic S stars observed by the Spitzer Space Telescope includes two sources with unusual low-contrast spectral structure between 7 and 14 mu m. The most likely estimate of the spectral continuum leads to the identification of molecular emission features from SiS at 7 and 13-14 mu m. The spectra also show what is best described as featureless excess emission, most likely from iron dust but possibly from amorphous carbon, as well as an emission feature from amorphous alumina dust peaking at 11-12 mu m. The spectra show long-wavelength excesses from cool dust grains in an extended envelope and additional emission features of unknown origin.
C1 [Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Hony, S.] Univ Paris 06, Lab AIM, CEA DSM CNRS, DAPNIA SAp, F-91191 Gif Sur Yvette, France.
[Smolders, K.; Decin, L.] Katholieke Univ Leuven, Inst Astron, Dept Phys & Astron, B-3001 Heverlee, Belgium.
[Zijlstra, A. A.] Univ Manchester, Sch Phys & Astron, Manchester M60 1QD, Lancs, England.
[Feast, M. W.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Feast, M. W.] Univ Cape Town, Gravitat Ctr, ZA-7701 Rondebosch, South Africa.
[Feast, M. W.; van Wyk, F.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[van Loon, J. Th.] Univ Keele, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Groenewegen, M. A. T.] Observ Royal Belgium, B-1180 Brussels, Belgium.
[Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sloan, GC (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM sloan@isc.astro.cornell.edu; sacha.hony@cea.fr;
kristof.smolders@ster.kuleuven.be; leen.decin@ster.kuleuven.be;
albert.zijlstra@manchester.ac.uk; mwf@ast.uct.ac.za; fvw@saao.ac.za;
jacco@astro.keele.ac.uk; marting@oma.be; sahai@jpl.nasa.gov
FU NASA [1407]; NASA through JPL [1257184]
FX We thank the anonymous referee, whose comments and questions helped us
improve this paper. We are also grateful to I. McDonald and D. Chernoff
for their valuable input concerning the contribution of dust to these
spectra. The observations were made with the Spitzer Space Telescope,
which is operated by JPL, California Institute of Technology under NASA
contract 1407 and supported by NASA through JPL (contract no. 1257184).
This research used the AAVSO International Database and the SIMBAD and
VIZIER databases, operated at the Centre de Donnees astronomiques de
Strasbourg.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
VL 729
IS 2
AR 121
DI 10.1088/0004-637X/729/2/121
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700044
ER
PT J
AU Wahhaj, Z
Liu, MC
Biller, BA
Clarke, F
Nielsen, EL
Close, LM
Hayward, TL
Mamajek, EE
Cushing, M
Dupuy, T
Tecza, M
Thatte, N
Chun, M
Ftaclas, C
Hartung, M
Reid, IN
Shkolnik, EL
Alencar, SHP
Artymowicz, P
Boss, A
Dal Pino, ED
Gregorio-Hetem, J
Ida, S
Kuchner, M
Lin, DNC
Toomey, DW
AF Wahhaj, Zahed
Liu, Michael C.
Biller, Beth A.
Clarke, Fraser
Nielsen, Eric L.
Close, Laird M.
Hayward, Thomas L.
Mamajek, Eric E.
Cushing, Michael
Dupuy, Trent
Tecza, Matthias
Thatte, Niranjan
Chun, Mark
Ftaclas, Christ
Hartung, Markus
Reid, I. Neill
Shkolnik, Evgenya L.
Alencar, Silvia H. P.
Artymowicz, Pawel
Boss, Alan
Dal Pino, Elisabethe de Gouveia
Gregorio-Hetem, Jane
Ida, Shigeru
Kuchner, Marc
Lin, Douglas N. C.
Toomey, Douglas W.
TI THE GEMINI NICI PLANET-FINDING CAMPAIGN: DISCOVERY OF A SUBSTELLAR L
DWARF COMPANION TO THE NEARBY YOUNG M DWARF CD-35 2722
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; instrumentation: adaptive optics; planetary systems;
planets and satellites: detection; stars: pre-main sequence
ID EXTRASOLAR GIANT PLANETS; FIELD SPECTROGRAPH NIFS; STAR ADAPTIVE OPTICS;
DORADUS MOVING GROUP; INFRARED FILTER SET; LOW-MASS STARS; BROWN DWARF;
T-DWARF; AB-DORADUS; SPECTROSCOPIC OBSERVATIONS
AB We present the discovery of a wide (67 AU) substellar companion to the nearby (21 pc) young solar-metallicity M1 dwarf CD-35 2722, a member of the approximate to 100 Myr AB Doradus association. Two epochs of astrometry from the NICI Planet-Finding Campaign confirm that CD-35 2722 B is physically associated with the primary star. Near-IR spectra indicate a spectral type of L4 +/- 1 with a moderately low surface gravity, making it one of the coolest young companions found to date. The absorption lines and near-IR continuum shape of CD-35 2722 B agree especially well the dusty field L4.5 dwarf 2MASS J22244381-0158521, while the near-IR colors and absolute magnitudes match those of the 5 Myr old L4 planetary-mass companion, 1RXS J160929.1-210524 b. Overall, CD-35 2722 B appears to be an intermediate-age benchmark for L dwarfs, with a less peaked H-band continuum than the youngest objects and near-IR absorption lines comparable to field objects. We fit Ames-Dusty model atmospheres to the near-IR spectra and find T-eff = 1700-1900 K and log(g) = 4.5 +/- 0.5. The spectra also show that the radial velocities of components A and B agree to within +/- 10 km s(-1), further confirming their physical association. Using the age and bolometric luminosity of CD-35 2722 B, we derive a mass of 31 +/- 8 M-Jup from the Lyon/Dusty evolutionary models. Altogether, young late-M to mid-L type companions appear to be overluminous for their near-IR spectral type compared with field objects, in contrast to the underluminosity of young late-L and early-T dwarfs.
C1 [Wahhaj, Zahed; Liu, Michael C.; Biller, Beth A.; Dupuy, Trent; Chun, Mark; Ftaclas, Christ] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Clarke, Fraser; Tecza, Matthias; Thatte, Niranjan] Univ Oxford, Dept Astron, DWB, Oxford OX1 3RH, England.
[Nielsen, Eric L.; Close, Laird M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Hayward, Thomas L.; Hartung, Markus] AURA, So Operat Ctr, Gemini Observ, La Serena, Chile.
[Mamajek, Eric E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Cushing, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Reid, I. Neill] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Shkolnik, Evgenya L.; Boss, Alan] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Alencar, Silvia H. P.] Univ Fed Minas Gerais, Dept Fis, ICEx, BR-30270901 Belo Horizonte, MG, Brazil.
[Artymowicz, Pawel] Univ Toronto Scarborough, Dept Phys & Environm Sci, Toronto, ON M1C 1A4, Canada.
[Dal Pino, Elisabethe de Gouveia; Gregorio-Hetem, Jane] Univ Sao Paulo, Dept Astron, IAG USP, BR-05508900 Sao Paulo, Brazil.
[Ida, Shigeru] Tokyo Inst Technol, Meguro Ku, Tokyo 1528550, Japan.
[Kuchner, Marc] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Lin, Douglas N. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Toomey, Douglas W.] Mauna Kea Infrared LLC, Hilo, HI 96720 USA.
RP Wahhaj, Z (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
RI Kuchner, Marc/E-2288-2012; Alencar, Silvia/C-2803-2013; 7,
INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Ida,
Shigeru/A-7840-2014; Gregorio-Hetem, Jane/A-5924-2013; de Gouveia Dal
Pino, Elisabete/H-9560-2013;
OI Ida, Shigeru/0000-0002-9676-3891; de Gouveia Dal Pino,
Elisabete/0000-0001-8058-4752; Biller, Beth/0000-0003-4614-7035;
Nielsen, Eric/0000-0001-6975-9056
FU NSF [AST-0713881, AST-0709484]
FX This work was supported in part by NSF grants AST-0713881 and
AST-0709484. Our research has employed the 2MASS data products; NASA's
Astrophysical Data System; the SIMBAD database operated at CDS,
Strasbourg, France; the M-, L-, and T-dwarf compendium housed at
DwarfArchives.org and maintained by Chris Gelino, Davy Kirkpatrick, and
Adam Burgasser; and the SpeX Prism Spectral Libraries maintained by Adam
Burgasser at http://www.browndwarfs.org/spexprism. We also thank Guillem
Anglada-Escude and Alycia Weinberger for their parallax measurements of
CD-35 2722 A.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
VL 729
IS 2
AR 139
DI 10.1088/0004-637X/729/2/139
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700062
ER
PT J
AU Whitmore, BC
Chandar, R
Kim, H
Kaleida, C
Mutchler, M
Stankiewicz, M
Calzetti, D
Saha, A
O'Connell, R
Balick, B
Bond, HE
Carollo, M
Disney, MJ
Dopita, MA
Frogel, JA
Hall, DNB
Holtzman, JA
Kimble, RA
McCarthy, PJ
Paresce, F
Silk, JI
Trauger, JT
Walker, AR
Windhorst, RA
Young, ET
AF Whitmore, Bradley C.
Chandar, Rupali
Kim, Hwihyun
Kaleida, Catherine
Mutchler, Max
Stankiewicz, Matt
Calzetti, Daniela
Saha, Abhijit
O'Connell, Robert
Balick, Bruce
Bond, Howard E.
Carollo, Marcella
Disney, Michael J.
Dopita, Michael A.
Frogel, Jay A.
Hall, Donald N. B.
Holtzman, Jon A.
Kimble, Randy A.
McCarthy, Patrick J.
Paresce, Francesco
Silk, Joseph I.
Trauger, John T.
Walker, Alistair R.
Windhorst, Rogier A.
Young, Erick T.
TI USING H alpha MORPHOLOGY AND SURFACE BRIGHTNESS FLUCTUATIONS TO AGE-DATE
STAR CLUSTERS IN M83
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M83); galaxies: star clusters: general; H II
regions; ISM: bubbles; stars: formation
ID SPECTRAL ENERGY-DISTRIBUTION; STELLAR POPULATION SYNTHESIS; MASSIVE
YOUNG CLUSTERS; LARGE-MAGELLANIC-CLOUD; GALAXIES NGC 4038/4039; FIELD
CAMERA 3; LUMINOSITY FUNCTION; INTERSTELLAR-MEDIUM; STARBURST GALAXIES;
GAS EXPULSION
AB We use new WFC3 observations of the nearby grand-design spiral galaxy M83 to develop two independent methods for estimating the ages of young star clusters. The first method uses the physical extent and morphology of H alpha emission to estimate the ages of clusters younger than tau approximate to 10 Myr. It is based on the simple premise that the gas in very young (tau < a few Myr) clusters is largely coincident with the cluster stars, is in a small, ring-like structure surrounding the stars in slightly older clusters since massive star winds and supernovae have had time to push out the natal gas (e.g., tau approximate to 5 Myr), and is in a larger ring-like bubble for still older clusters (i.e., approximate to 5-10 Myr). If no H alpha is associated with a cluster it is generally older than approximate to 10 Myr. The second method is based on an observed relation between pixel-to-pixel flux variations within clusters and their ages. This method relies on the fact that the brightest individual stars in a cluster are most prominent at ages around 10 Myr, and fall below the detection limit (i.e., M-V < -3.5) for ages older than about 100 Myr. Older clusters therefore have a smoother appearance and smaller pixel-to-pixel variations. The youngest clusters also have lower flux variations, hence the relationship is double valued. This degeneracy in age can be broken using other age indicators such as H alpha morphology. These two methods are the basis for a new morphological classification system which can be used to estimate the ages of star clusters based on their appearance. We compare previous age estimates of clusters in M83 determined from fitting UBVIH alpha measurements using predictions from stellar evolutionary models with our new morphological categories and find good agreement, at the approximate to 95% level. The scatter within categories is approximate to 0.1 dex in log tau for young clusters (< 10 Myr) and approximate to 0.5 dex for older (> 10 Myr) clusters. A by-product of this study is the identification of 22 "single-star" H II regions in M83, with central stars having ages approximate to 4 Myr.
C1 [Whitmore, Bradley C.; Mutchler, Max; Stankiewicz, Matt; Bond, Howard E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Chandar, Rupali] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Kim, Hwihyun; Kaleida, Catherine; Windhorst, Rogier A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[O'Connell, Robert] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Carollo, Marcella] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Disney, Michael J.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Frogel, Jay A.] AURA, Washington, DC 20005 USA.
[Hall, Donald N. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCarthy, Patrick J.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Paresce, Francesco] INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy.
[Silk, Joseph I.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Trauger, John T.] NASA JPL, Pasadena, CA 91109 USA.
[Walker, Alistair R.] Cerro Tololo Interamer Observ, La Serena, Chile.
[Young, Erick T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Whitmore, BC (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM whitmore@stsci.edu
RI Dopita, Michael/P-5413-2014
OI Dopita, Michael/0000-0003-0922-4986
FU NASA [NAS5-26555]; NSF [0847467]
FX We thank Zolt Levay for making the color images used in Figures 1 and 2.
This paper is based on observations taken with the NASA/ESA Hubble Space
Telescope obtained at the Space Telescope Science Institute, which is
operated by AURA, Inc., under NASA contract NAS5-26555. The paper makes
use of Early Release Science observations made by the WFC3 Science
Oversight Committee. We are grateful to the Director of STScI for
awarding Director's Discretionary time for this program. R.C. is
grateful for support from NSF through CAREER award 0847467. 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 NASA.
NR 36
TC 36
Z9 36
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2011
VL 729
IS 2
AR 78
DI 10.1088/0004-637X/729/2/78
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 737ZI
UT WOS:000288608700001
ER
PT J
AU Xie, Y
Yang, P
Kattawar, GW
Baum, BA
Hu, YX
AF Xie, Yu
Yang, Ping
Kattawar, George W.
Baum, Bryan A.
Hu, Yongxiang
TI Simulation of the optical properties of plate aggregates for application
to the remote sensing of cirrus clouds
SO APPLIED OPTICS
LA English
DT Article
ID SINGLE-SCATTERING PROPERTIES; DISCRETE-DIPOLE APPROXIMATION;
SATELLITE-BASED RETRIEVAL; SHAPED ICE CRYSTALS; LIGHT-SCATTERING;
SURFACE-ROUGHNESS; MICROPHYSICAL CHARACTERISTICS; RADIATIVE-TRANSFER;
BULLET ROSETTES; PARTICLE-SIZE
AB In regions of deep tropical convection, ice particles often undergo aggregation and form complex chains. To investigate the effect of the representation of aggregates on electromagnetic scattering calculations, we developed an algorithm to efficiently specify the geometries of aggregates and to compute some of their geometric parameters, such as the projected area. Based on in situ observations, ice aggregates are defined as clusters of hexagonal plates with a chainlike overall shape, which may have smooth or roughened surfaces. An aggregate representation is developed with 10 ensemble members, each consisting of between 4-12 hexagonal plates. The scattering properties of an individual aggregate ice particle are computed using either the discrete dipole approximation or an improved geometric optics method, depending upon the size parameters. Subsequently, the aggregate properties are averaged over all geometries. The scattering properties of the aggregate representation closely agree with those computed from 1000 different aggregate geometries. As a result, the aggregate representation provides an accurate and computationally efficient way to represent all aggregates occurring within ice clouds. Furthermore, the aggregate representation can be used to study the influence of these complex ice particles on the satellite-based remote sensing of ice clouds. The computed cloud reflectances for aggregates are different from those associated with randomly oriented individual hexagonal plates. When aggregates are neglected, simulated cloud reflectances are generally lower at visible and shortwave-infrared wavelengths, resulting in smaller effective particle sizes but larger optical thicknesses. (C) 2011 Optical Society of America
C1 [Xie, Yu; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Kattawar, George W.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Baum, Bryan A.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Xie, Y (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM xieyupku@tamu.edu
RI Yang, Ping/B-4590-2011; Xie, Yu/A-4266-2011; Hu, Yongxiang/K-4426-2012;
Baum, Bryan/B-7670-2011
OI Baum, Bryan/0000-0002-7193-2767
FU National Aeronautics and Space Administration (NASA) [NNX08AF68G,
NNX08AF81G]; University of Wisconsin [G074605]; Office of Naval Research
(ONR) [N00014-06-1-0069]
FX This research is supported by a research grant from National Aeronautics
and Space Administration (NASA) (NNX08AF68G) from the NASA Radiation
Sciences Program managed by Hal Maring and the MODIS Program managed by
Paula Bontempi. This study was also partly supported by a subcontract
G074605 issued by the University of Wisconsin to Texas A&M University.
George W. Kattawar's research is also supported by the Office of Naval
Research (ONR) under contract N00014-06-1-0069. Bryan Baum gratefully
acknowledges the support provided through NASA grant NNX08AF81G.
NR 59
TC 15
Z9 15
U1 0
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD MAR 10
PY 2011
VL 50
IS 8
BP 1065
EP 1081
DI 10.1364/AO.50.001065
PG 17
WC Optics
SC Optics
GA 732QP
UT WOS:000288204100001
PM 21394178
ER
PT J
AU Tseng, WL
Johnson, RE
Thomsen, MF
Cassidy, TA
Elrod, MK
AF Tseng, Wei-Ling
Johnson, Robert E.
Thomsen, Michelle F.
Cassidy, Timothy A.
Elrod, Meredith K.
TI Neutral H-2 and H-2(+) ions in the Saturnian magnetosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MOLECULAR-HYDROGEN; TITANS ATMOSPHERE; CROSS-SECTIONS; ICY MOON;
ENCELADUS; RINGS; PLASMA; CLOUD; MODEL; SATELLITES
AB The Saturnian system is immersed in an extended cloud of neutrals. Although water vapor ejected from Enceladus' south pole is the dominant neutral source, photolysis and radiolysis of ices can release H2O, O-2, and H-2 from the icy ring particles and the icy satellites, and Titan's atmosphere is a source of H-2. Once ionized, these neutrals are the source of the observed magnetospheric plasma. To understand the H-2(+) ion densities observed by the Cassini plasma spectrometer (CAPS), we developed a Monte Carlo test particle model to simulate the spatial morphology of the neutral H-2 cloud and the resulting H-2(+) ion source rates. The H-2 lifetime is constrained by its local chemistry, which is computed from the latest plasma measurements by Cassini CAPS data. The main rings, Enceladus' water torus, Rhea, and Titan are considered as the primary sources of H-2 in our model. It is seen that H-2 accumulates over Saturn's main rings because of thermal accommodation with the ring particles, and Titan is the dominant source of H-2 in the outer magnetosphere (>similar to 6 RS). From similar to 6 to similar to 2.5 RS, photodissociation of water from Enceladus and H-2 scattered from the ring atmosphere are comparable sources. The newly formed H-2(+) ions are lost by collisions with the ring particles inside similar to 2.5 R-S, by interchange processes in the middle magnetosphere, and by flow down the tail in the outer magnetosphere. The density distribution of H-2(+) estimated from our ion source rates roughly agrees with CAPS observations, and we show that the H-2(+) density near the equator over the main rings is at least 1 order of magnitude smaller than O-2(+), possibly consistent with the nondetection of H-2(+) by CAPS at Saturn orbit insertion.
C1 [Tseng, Wei-Ling; Johnson, Robert E.; Elrod, Meredith K.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22903 USA.
[Cassidy, Timothy A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Thomsen, Michelle F.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Tseng, WL (reprint author), Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22903 USA.
EM wt7b@virginia.edu
FU NASA; U.S. Department of Energy
FX We thank H. T. Smith and A. Rymer for useful discussions and comments.
This work is supported by a grant from NASA's Planetary Atmosphere's
Program and by a NASA Cassini data analysis grant. Work at Los Alamos
was conducted under the auspices of the U.S. Department of Energy with
funding from NASA's Cassini project.
NR 74
TC 12
Z9 12
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 MAR 9
PY 2011
VL 116
AR A03209
DI 10.1029/2010JA016145
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 734JS
UT WOS:000288331000004
ER
PT J
AU Lee, JN
Wu, DL
Manney, GL
Schwartz, MJ
Lambert, A
Livesey, NJ
Minschwaner, KR
Pumphrey, HC
Read, WG
AF Lee, Jae N.
Wu, Dong L.
Manney, Gloria L.
Schwartz, Michael J.
Lambert, Alyn
Livesey, Nathaniel J.
Minschwaner, Kenneth R.
Pumphrey, Hugh C.
Read, William G.
TI Aura Microwave Limb Sounder observations of the polar middle atmosphere:
Dynamics and transport of CO and H2O
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CARBON-MONOXIDE; WATER-VAPOR; STRATOSPHERIC TRANSPORT; INTERANNUAL
VARIABILITY; SOUTHERN-HEMISPHERE; ARCTIC OSCILLATION; LOWER MESOSPHERE;
ANNULAR MODES; ACE-FTS; PART I
AB The vertical structure and evolution of the wintertime annular modes are studied using 6 years of geopotential height, carbon monoxide (CO), and water vapor (H2O) data from Aura Microwave Limb Sounder. The Northern Hemisphere annular mode (NAM) and the Southern Hemisphere annular mode (SAM) reveal a strong coupling of the dynamics in the stratosphere and mesosphere between 316 hPa (similar to 9 km) and 0.002 hPa (similar to 90 km). CO is a good tracer throughout the middle atmosphere, while variable vertical gradients of H2O limit the regions where it is useful as a dynamical tracer. The maximum of the CO NAM and SAM (CNAM and CSAM) indices is used to monitor and characterize the evolution of wintertime polar dynamics as a function of time and height. The CNAM analysis reveals reformation of a stronger mesospheric polar vortex after significant stratospheric sudden warmings in 2006, 2009, and 2010. There is a significant anticorrelation between the mesospheric and stratospheric CNAM indices during 2005-2010 winters, supporting the hypothesis of mesosphere-stratosphere coupling through planetary-gravity wave interactions.
C1 [Lee, Jae N.; Wu, Dong L.; Manney, Gloria L.; Schwartz, Michael J.; Lambert, Alyn; Livesey, Nathaniel J.; Read, William G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Manney, Gloria L.; Minschwaner, Kenneth R.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Pumphrey, Hugh C.] Univ Edinburgh, Inst Atmospher & Environm Sci, Sch GeoSci, Edinburgh EH9 3JN, Midlothian, Scotland.
RP Lee, JN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jae.nyung.lee@jpl.nasa.gov
RI Schwartz, Michael/F-5172-2016; Wu, Dong/D-5375-2012
OI Schwartz, Michael/0000-0001-6169-5094;
FU MLS; NASA
FX We thank the MLS science team for their support. We also thank Varat
Limpasuvan, Hanli Liu, Kunihiro Kodera, Alexander Ruzmaikin, and Joan
Feynman for inspiring discussions. We would also like to acknowledge
three anonymous reviewers who helped significantly improve the paper and
whose comments we have adapted in the discussion. This research was
supported by an appointment to the NASA Postdoctoral Program at the Jet
Propulsion Laboratory, administered by Oak Ridge Associated Universities
through a contract with NASA. The work at the Jet Propulsion Laboratory,
California Institute of Technology, was conducted under contract with
the National Aeronautics and Space Administration.
NR 61
TC 27
Z9 29
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 8
PY 2011
VL 116
AR D05110
DI 10.1029/2010JD014608
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 734HH
UT WOS:000288324700002
ER
PT J
AU Huang, CS
de la Beaujardiere, O
Roddy, PA
Hunton, DE
Pfaff, RF
Valladares, CE
Ballenthin, JO
AF Huang, Chao-Song
de la Beaujardiere, O.
Roddy, P. A.
Hunton, D. E.
Pfaff, R. F.
Valladares, C. E.
Ballenthin, J. O.
TI Evolution of equatorial ionospheric plasma bubbles and formation of
broad plasma depletions measured by the C/NOFS satellite during deep
solar minimum
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GRAVITY-WAVE INITIATION; BOTTOMSIDE F-LAYER; SPREAD-F; NONLINEAR
EVOLUTION; BACKSCATTER PLUMES; IRREGULARITIES; GENERATION; REGION;
CAMPAIGN; DRIFTS
AB An unexpected feature revealed by the measurements of the Communication/Navigation Outage Forecasting System (C/NOFS) satellite is the presence of broad plasma depletions in the midnight-dawn sector during deep solar minimum. It has not been well understood what causes the broad plasma depletions and how equatorial plasma bubbles are related to the broad depletions. In this paper we present the C/NOFS measurements of equatorial plasma bubbles and broad depletions in a few cases. The ion density perturbations and enhanced ion vertical velocity are first identified in the topside F region at similar to 2200 LT, suggesting that the plasma bubbles start to form earlier at lower altitudes. The observations show that the plasma bubbles observed in the midnight-dawn sector may originate in the evening sector. The plasma bubbles continue growing for more than 3.3 h, and the decay time of the bubbles is also longer than 3.3 h. The continuous growth of the plasma bubbles in the evening sector and the slow decay after midnight determine that most plasma bubbles become fully developed and are easily detected in the midnight-dawn sector. The plasma flow inside the bubbles remains strongly upward throughout the entire nighttime. We propose the following mechanism for the generation of wide plasma bubbles and broad depletions. A series of plasma bubbles is generated through the Rayleigh-Taylor instability process over a large longitudinal range. These plasma bubbles grow and merge to form a wide bubble (width of similar to 700 km as observed), and multiple regular and/or wide bubbles can further merge to form broad plasma depletions (thousands of kilometers in longitude). The ion vertical drift inside each plasma bubble is driven by the polarization electric field and remains large after the bubbles have merged. This mechanism provides a reasonable interpretation of the large upward ion drift velocity inside the broad depletion region.
C1 [Huang, Chao-Song; Valladares, C. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA.
[de la Beaujardiere, O.; Roddy, P. A.; Hunton, D. E.; Ballenthin, J. O.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA.
[Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Huang, CS (reprint author), Boston Coll, Inst Sci Res, 402 St Clements Hall,140 Commonwealth Ave, Chestnut Hill, MA 02467 USA.
EM chaosong.huang.ctr@hanscom.af.mil
RI Pfaff, Robert/F-5703-2012
OI Pfaff, Robert/0000-0002-4881-9715
FU Air Force Office of Scientific Research [FA9550-09-1-0321]; Air Force
Research Laboratory; Department of Defense; National Aeronautics and
Space Administration; Naval Research Laboratory; Aerospace Corporation
FX Work by C. S. H. was supported by the Air Force Office of Scientific
Research award FA9550-09-1-0321. The C/NOFS mission is supported by the
Air Force Research Laboratory, the Department of Defense Space Test
Program, the National Aeronautics and Space Administration, the Naval
Research Laboratory, and the Aerospace Corporation.
NR 59
TC 23
Z9 23
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR 8
PY 2011
VL 116
AR A03309
DI 10.1029/2010JA015982
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 734JR
UT WOS:000288330900002
ER
PT J
AU Zhang, JY
Wu, LY
Huang, G
Zhu, WQ
Zhang, Y
AF Zhang, Jingyong
Wu, Lingyun
Huang, Gang
Zhu, Wenquan
Zhang, Yan
TI The role of May vegetation greenness on the southeastern Tibetan Plateau
for East Asian summer monsoon prediction
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LAND-COVER CHANGE; EURASIAN SNOW COVER; SOIL-MOISTURE; EL-NINO;
STATISTICAL-ANALYSIS; SURFACE-TEMPERATURE; CLIMATE FEEDBACKS; REGIONAL
CLIMATE; UNITED-STATES; RAINFALL
AB It is well known that the slowly varying oceanic processes provide the primary source for East Asian summer monsoon (EASM) predictability. However, the memory inherent in the land surface state is less well understood or applied toward the EASM prediction. Here we investigate the role of antecedent vegetation conditions over East Asia for the EASM variation and prediction using March, April, May, and spring mean satellite-sensed Normalized Difference Vegetation Index (NDVI) for the period of 1982-2006. Results show that May vegetation greenness on the southeastern Tibetan Plateau (TP) is most closely linked to the EASM, accounting for about half of the total EASM variance. May vegetation greenness on the southeastern TP has significant and positive correlations with summer rainfall over the southeastern TP, East Asian summer subtropical frontal region, and many areas of northern China. We further discuss the possible physical mechanism explaining our findings. It is proposed that increased TP vegetation greenness enhances surface thermal effects, which subsequently warm atmospheric temperature, as well as strengthen ascending motion, convergence at the lower layers and divergence at the higher layers, and summer monsoon circulation. Finally, a linear regression model is developed to predict the EASM strength by combination of El Nino-Southern Oscillation (ENSO) and the vegetation greenness. Hindcast for the period 1982-2006 shows that the use of the southeastern TP vegetation information can highly improve the EASM prediction skill compared to that using ENSO alone.
C1 [Zhang, Jingyong; Wu, Lingyun] Chinese Acad Sci, Ctr Monsoon Syst Res, Inst Atmospher Phys, Beijing 100029, Peoples R China.
[Huang, Gang] Chinese Acad Sci, Inst Atmospher Phys, LASG, Beijing 100029, Peoples R China.
[Huang, Gang] Chinese Acad Sci, Inst Atmospher Phys, RCE TEA, Beijing 100029, Peoples R China.
[Zhu, Wenquan] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China.
[Zhang, Yan] Univ Maryland Baltimore Cty, GEST, Catonsville, MD 21228 USA.
[Zhang, Yan] NASA, Climate & Radiat Branch, Greenbelt, MD USA.
RP Zhang, JY (reprint author), Chinese Acad Sci, Ctr Monsoon Syst Res, Inst Atmospher Phys, Beijing 100029, Peoples R China.
EM zjy@mail.iap.ac.cn
RI Zhang, Jingyong/B-8849-2011; li, dongsheng/B-2285-2012; Zhang,
Yan/C-4792-2012
FU U.S. National Weather Service; PCMDI (U.S. Department of Energy);
Chinese Academy of Sciences; Chinese Academy; National Basic Research
Program of China [2009CB421405]
FX The source for NDVI data set was the Global Land Cover Facility,
University of Maryland. NCEP/DOE reanalysis was produced with the
support of the U.S. National Weather Service and of PCMDI (U.S.
Department of Energy). This work was supported by the "100-talent
program" of the Chinese Academy of Sciences, a special fund for the
President's prize of the Chinese Academy of, and National Basic Research
Program of China (2009CB421405).
NR 97
TC 8
Z9 9
U1 2
U2 17
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 MAR 5
PY 2011
VL 116
AR D05106
DI 10.1029/2010JD015095
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 731EB
UT WOS:000288088000003
ER
PT J
AU Matsui, H
Kondo, Y
Moteki, N
Takegawa, N
Sahu, LK
Zhao, Y
Fuelberg, HE
Sessions, WR
Diskin, G
Blake, DR
Wisthaler, A
Koike, M
AF Matsui, H.
Kondo, Y.
Moteki, N.
Takegawa, N.
Sahu, L. K.
Zhao, Y.
Fuelberg, H. E.
Sessions, W. R.
Diskin, G.
Blake, D. R.
Wisthaler, A.
Koike, M.
TI Seasonal variation of the transport of black carbon aerosol from the
Asian continent to the Arctic during the ARCTAS aircraft campaign
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LASER-INDUCED INCANDESCENCE; LONG-TERM TRENDS; AIR-POLLUTION; GLOBAL
PRECIPITATION; INTERANNUAL VARIABILITY; TROPOSPHERIC AEROSOL; ART.;
SMOKE; MONOXIDE; PACIFIC
AB Extensive measurements of black carbon (BC) aerosol were conducted in and near the North American Arctic during the Arctic Research of the Composition of the Troposphere from Aircraft and Satellites (ARCTAS) aircraft campaign in April and June-July 2008. We identify the pathways and mechanisms of transport of BC to the Arctic from the Asian continent using these data. The concentration, transport efficiency, and measured altitude of BC over the North American Arctic were highly dependent on season and origin of air parcels, e.g., biomass burning (BB) in Russia (Russian BB) and anthropogenic (AN) in East Asia (Asian AN). Russian BB air was mainly measured in the middle troposphere and caused maximum BC concentrations at this altitude in spring. The median BC concentration and transport efficiency of the Russian BB air were 270 ng m(-3) (at STP) and 80% in spring and 20 ng m(-3) and 4% in summer, respectively. Asian AN air was measured most frequently in the upper troposphere, with median values of 20 ng m(-3) and 13% in spring and 5 ng m(-3) and 0.8% in summer. These distinct differences are explained by differences in the transport mechanisms and accumulated precipitation along trajectories (APT), which is a measure of wet removal processes during transport. The transport of Russian BB air to the Arctic was nearly isentropic with slow ascent (low APT), while Asian AN air underwent strong uplift associated with warm conveyor belts (high APT). The APT values in summer were much larger than those in spring due to the increase in humidity in summer. These results show that the impact of BC emitted from AN sources in East Asia on the Arctic was very limited in both spring and summer. The BB emissions in Russia in spring are demonstrated to be the most important sources of BC transported to the North American Arctic.
C1 [Matsui, H.] Univ Tokyo, Adv Sci & Technol Res Ctr, Meguro Ku, Tokyo 1538904, Japan.
[Sahu, L. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India.
[Zhao, Y.] Univ Calif Davis, Air Qual Res Ctr, Davis, CA 95616 USA.
[Fuelberg, H. E.; Sessions, W. R.] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
[Diskin, G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Blake, D. R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA.
[Wisthaler, A.] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria.
[Koike, M.] Univ Tokyo, Dept Earth & Planetary Sci, Grad Sch Sci, Bunkyo Ku, Tokyo 1130033, Japan.
RP Matsui, H (reprint author), Univ Tokyo, Adv Sci & Technol Res Ctr, Meguro Ku, 4-6-1 Komaba, Tokyo 1538904, Japan.
EM matsui@atmos.rcast.u-tokyo.ac.jp; y.kondo@atmos.rcast.u-tokyo.ac.jp;
moteki@atmos.rcast.u-tokyo.ac.jp; takegawa@atmos.rcast.u-tokyo.ac.jp;
lokesh@prl.res.in; yjzhao@ucdavis.edu; hfuelberg@fsu.edu;
walter.sessions@gmail.com; glenn.s.diskin@nasa.gov; drblake@uci.edu;
armin.wisthaler@uibk.ac.at; koike@eps.s.u-tokyo.ac.jp
RI Koike, Makoto/F-4366-2011; Kondo, Yutaka/D-1459-2012; Sessions,
Walter/O-8096-2014
OI Sessions, Walter/0000-0002-5376-4894
FU NASA [USP-SMD-08-009]; Ministry of Education, Culture, Sports, Science,
and Technology (MEXT); Japan Science and Technology Agency (JST);
Japanese Ministry of the Environment [B-083]; Austrian Research
Promotion Agency; Tiroler Zukunftstiftung
FX The ARCTAS campaign 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. 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). Y.Z. was supported in part by NASA Tropospheric Chemistry
Program (USP-SMD-08-009). CH3CN measurements were supported
by the Austrian Research Promotion Agency (FFG-ALR) and the Tiroler
Zukunftstiftung and carried out with the help/support of T. Mikoviny, M.
Graus, A. Hansel, and T. D. Maerk.
NR 73
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U1 6
U2 25
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 MAR 5
PY 2011
VL 116
AR D05202
DI 10.1029/2010JD015067
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 731EB
UT WOS:000288088000002
ER
PT J
AU Witt, CJ
Richards, AL
Masuoka, PM
Foley, DH
Buczak, AL
Musila, LA
Richardson, JH
Colacicco-Mayhugh, MG
Rueda, LM
Klein, TA
Anyamba, A
Small, J
Pavlin, JA
Fukuda, MM
Gaydos, J
Russell, KL
AF Witt, Clara J.
Richards, Allen L.
Masuoka, Penny M.
Foley, Desmond H.
Buczak, Anna L.
Musila, Lillian A.
Richardson, Jason H.
Colacicco-Mayhugh, Michelle G.
Rueda, Leopoldo M.
Klein, Terry A.
Anyamba, Assaf
Small, Jennifer
Pavlin, Julie A.
Fukuda, Mark M.
Gaydos, Joel
Russell, Kevin L.
CA AFHSC-GEIS Predictive Surveillance
TI The AFHSC-Division of GEIS Operations Predictive Surveillance Program: a
multidisciplinary approach for the early detection and response to
disease outbreaks
SO BMC PUBLIC HEALTH
LA English
DT Review
ID REPUBLIC-OF-KOREA; RIFT-VALLEY; CUTANEOUS LEISHMANIASIS; BARINGO
DISTRICT; UNITED-STATES; GEOGRAPHIC DISTRIBUTIONS; VISCERAL
LEISHMANIASIS; CLIMATE-CHANGE; KENYA; HANTAVIRUS
AB The Armed Forces Health Surveillance Center, Division of Global Emerging Infections Surveillance and Response System Operations (AFHSC-GEIS) initiated a coordinated, multidisciplinary program to link data sets and information derived from eco-climatic remote sensing activities, ecologic niche modeling, arthropod vector, animal disease-host/reservoir, and human disease surveillance for febrile illnesses, into a predictive surveillance program that generates advisories and alerts on emerging infectious disease outbreaks. The program's ultimate goal is pro-active public health practice through pre-event preparedness, prevention and control, and response decision-making and prioritization. This multidisciplinary program is rooted in over 10 years experience in predictive surveillance for Rift Valley fever outbreaks in Eastern Africa. The AFHSC-GEIS Rift Valley fever project is based on the identification and use of disease-emergence critical detection points as reliable signals for increased outbreak risk. The AFHSC-GEIS predictive surveillance program has formalized the Rift Valley fever project into a structured template for extending predictive surveillance capability to other Department of Defense (DoD)-priority vector-and water-borne, and zoonotic diseases and geographic areas. These include leishmaniasis, malaria, and Crimea-Congo and other viral hemorrhagic fevers in Central Asia and Africa, dengue fever in Asia and the Americas, Japanese encephalitis (JE) and chikungunya fever in Asia, and rickettsial and other tick-borne infections in the U. S., Africa and Asia.
C1 [Witt, Clara J.; Fukuda, Mark M.; Gaydos, Joel; Russell, Kevin L.] USAF, Hlth Surveillance Ctr, Silver Spring, MD 20910 USA.
[Richards, Allen L.] USN, Med Res Ctr, Dept Rickettsial Dis Res Program, Silver Spring, MD 20910 USA.
[Richards, Allen L.; Masuoka, Penny M.] Uniformed Serv Univ Hlth Sci, Dept Prevent Med & Biometr, Bethesda, MD 20814 USA.
[Foley, Desmond H.; Colacicco-Mayhugh, Michelle G.; Rueda, Leopoldo M.] Walter Reed Army Inst Res, Walter Reed Biosystemat Unit, Div Entomol, Silver Spring, MD 20910 USA.
[Buczak, Anna L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Musila, Lillian A.] Kenya Govt Med Res Ctr, Ctr Virus Res, Nairobi, Kenya.
[Musila, Lillian A.] USA, Med Res Unit Kenya, Nairobi Unit 64109, APO, AE 09831 USA.
[Richardson, Jason H.; Pavlin, Julie A.] Armed Forces Res Inst Med Sci, Bangkok 10400, Thailand.
[Klein, Terry A.] Force Hlth Protect & Prevent Med, Med Brigade 65, Unit 15281, APO, AP 96205 USA.
[Anyamba, Assaf; Small, Jennifer] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, GIMMS Grp, Greenbelt, MD 20771 USA.
USN, Portsmouth, VA 23708 USA.
Marine Corps Public Hlth Ctr, Portsmouth, VA 23708 USA.
USDA, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA.
Naval Med Res Unit 3, Cairo 11517, Egypt.
USA, Med Res Unit Kenya, Dept Entomol & Vector Borne Dis, Kisumu Unit 8900, APO, AE 09831 USA.
[AFHSC-GEIS Predictive Surveillance] Komplek P2M PLP LITBANGKES JI, Naval Med Res Unit 2, Jakarta 10560, Indonesia.
US Naval Med Res Ctr Detachment, Ctr Med Naval CEMENA, Lima, Peru.
Walter Reed Army Inst Res, Div Prevent Med, Silver Spring, MD 20910 USA.
RP Witt, CJ (reprint author), USAF, Hlth Surveillance Ctr, 503 Robert Grant Ave, Silver Spring, MD 20910 USA.
EM clara.witt@us.army.mil
RI Richardson, Jason/A-9441-2011; Valle, Ruben/A-7512-2013;
OI Foley, Desmond/0000-0001-7525-4601
NR 48
TC 7
Z9 7
U1 3
U2 28
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2458
J9 BMC PUBLIC HEALTH
JI BMC Public Health
PD MAR 4
PY 2011
VL 11
SU 2
AR S10
DI 10.1186/1471-2458-11-S2-S10
PG 16
WC Public, Environmental & Occupational Health
SC Public, Environmental & Occupational Health
GA 759WT
UT WOS:000290279900010
PM 21388561
ER
PT J
AU Mach, DM
Blakeslee, RJ
Bateman, MG
AF Mach, Douglas M.
Blakeslee, Richard J.
Bateman, Monte G.
TI Global electric circuit implications of combined aircraft storm electric
current measurements and satellite-based diurnal lightning statistics
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL TRANSIENT DETECTOR; IMAGING SENSOR; THUNDERSTORMS; FIELD;
ELECTRIFICATION; CALIBRATION; PLATFORMS
AB We have combined analyses of high-altitude aircraft observations of electrified clouds with diurnal lightning statistics from the Lightning Imaging Sensor (LIS) and Optical Transient Detector (OTD) that are carried aboard low-Earth-orbiting satellites to reproduce the diurnal variation in the global electric circuit. Using basic assumptions about the mean storm currents as a function of flash rate and location (i.e., land or ocean) and the global electric circuit, our estimate of the current in the global electric circuit matches the Carnegie curve diurnal variation to within 4% for all but two short periods of time, in which the difference was 11% in one time period (0430 UTC) and 6% in the second period (1830 UTC). This excellent agreement with the Carnegie curve was obtained without any tuning or adjustment of the satellite or aircraft data. We assume that (1) the mean values for current and flash rates in the aircraft storm overflight data set (1.7 A and 0.8 flashes min(-1) for oceanic thunderstorms, 1.0 A and 2.2 flashes min(-1) for land thunderstorms, 0.41 A for oceanic electrified shower clouds (i.e., electrified but no lightning detected), and 0.13 A for land electrified shower clouds) and (2) the diurnal variations in lightning rates over land and ocean found in the satellite data set are universally applicable. Mean contributions to the global electric circuit from land and ocean thunderstorms are 1.1 kA (land) and 0.7 kA (ocean). Contributions to the global electric circuit from electrified shower clouds are 0.22 kA for ocean storms and 0.04 kA for land storms. The mean total conduction current for the global electric circuit is 2.0 kA. The means that for the number of storms contributing to the global electric circuit, 1100 are land storms with lightning, 530 are ocean storms without lightning, 390 are ocean storms with lightning, and 330 are land storms without lightning. A closer fit to the Carnegie curve is possible if the contributions from electrified shower clouds are increased by a factor of 3 or 4.
C1 [Mach, Douglas M.] Univ Alabama, Global Hydrol & Climate Ctr, Huntsville, AL 35899 USA.
[Bateman, Monte G.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Blakeslee, Richard J.] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
RP Mach, DM (reprint author), Univ Alabama, Global Hydrol & Climate Ctr, Huntsville, AL 35899 USA.
EM dmach@nasa.gov
FU NASA's Earth Science Enterprise (ESE); NASA
FX The authors gratefully thank NASA's Earth Science Enterprise (ESE) and
program managers Ramesh Kakar (ER-2, general data analysis) and Cheryl
Yuhas (Altus) for support of this research. The aircraft data used in
this study were acquired during flight campaigns supported by NASA's
Research and Technology Operating Plan (RTOP) and Research Opportunities
in Space and Earth Science (ROSES) awards, Earth Observing System (EOS)
support (for general data analysis), and the Uninhabited Aerial Vehicle
Science Demonstration Project (UAV SDP). We would like to thank Charles
Croskey for providing the conductivity data from the ACES project. Data
used in this study were taken from the LIS-OTD gridded climatologies,
available for order from the Global Hydrology Resource Center
(http://ghrc.msfc.nasa.gov). The LIS-OTD instrument team was funded by
the NASA Earth Science Enterprise (ESE) Earth Observing System (EOS)
project.
NR 33
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U1 0
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 MAR 4
PY 2011
VL 116
AR D05201
DI 10.1029/2010JD014462
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 731DZ
UT WOS:000288087800002
ER
PT J
AU Howett, CJA
Spencer, JR
Pearl, J
Segura, M
AF Howett, C. J. A.
Spencer, J. R.
Pearl, J.
Segura, M.
TI High heat flow from Enceladus' south polar region measured using 10-600
cm(-1) Cassini/CIRS data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID BOLOMETRIC ALBEDOS; ENERGY-BALANCE; LIQUID WATER; E-RING; SURFACE;
ORIGIN; SATURN; IO; FRACTURES; MODELS
AB Analysis of 2008 Cassini Composite Infrared Spectrometer (CIRS) 10 to 600 cm(-1) thermal emission spectra of Encleadus shows that for reasonable assumptions about the spatial distribution of the emission and the thermophysical properties of the solar-heated background surface, which are supported by CIRS observations of background temperatures at the edge of the active region, the endogenic power of Enceladus' south polar terrain is 15.8 +/- 3.1 GW. This is significantly higher than the previous estimate of 5.8 +/- 1.9 GW. The new value represents an improvement over the previous one, which was derived from higher wave number data (600 to 1100 cm(-1)) and was thus only sensitive to high-temperature emission. The mechanism capable of producing such a high endogenic power remains a mystery and challenges the current models of proposed heat production.
C1 [Howett, C. J. A.; Spencer, J. R.] SW Res Inst, Boulder, CO 80302 USA.
[Pearl, J.; Segura, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Howett, CJA (reprint author), SW Res Inst, 1050 Walnut St,Ste 300, Boulder, CO 80302 USA.
EM howett@boulder.swri.edu
FU Cassini project; NASA [NNG06GF41G, NNX07AU40G]
FX Thanks are due to the Cassini project and especially the CIRS team that
made these data possible. This work was supported by the Cassini project
and NASA grants NNG06GF41G and NNX07AU40G.
NR 34
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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 MAR 4
PY 2011
VL 116
AR E03003
DI 10.1029/2010JE003718
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 731CW
UT WOS:000288084900002
ER
PT J
AU Talukder, D
Mitra, S
Bose, S
AF Talukder, Dipongkar
Mitra, Sanjit
Bose, Sukanta
TI Multibaseline gravitational wave radiometry
SO PHYSICAL REVIEW D
LA English
DT Article
ID RESOLUTION; SEARCHES; NETWORK; VIRGO
AB We present a statistic for the detection of stochastic gravitational wave backgrounds (SGWBs) using radiometry with a network of multiple baselines. We also quantitatively compare the sensitivities of existing baselines and their network to SGWBs. We assess how the measurement accuracy of signal parameters, e. g., the sky position of a localized source, can improve when using a network of baselines, as compared to any of the single participating baselines. The search statistic itself is derived from the likelihood ratio of the cross correlation of the data across all possible baselines in a detector network and is optimal in Gaussian noise. Specifically, it is the likelihood ratio maximized over the strength of the SGWB and is called the maximized-likelihood ratio (MLR). One of the main advantages of using the MLR over past search strategies for inferring the presence or absence of a signal is that the former does not require the deconvolution of the cross correlation statistic. Therefore, it does not suffer from errors inherent to the deconvolution procedure and is especially useful for detecting weak sources. In the limit of a single baseline, it reduces to the detection statistic studied by Ballmer [Classical Quantum Gravity 23, S179 (2006).] and Mitra et al. [Phys. Rev. D 77, 042002 (2008).]. Unlike past studies, here the MLR statistic enables us to compare quantitatively the performances of a variety of baselines searching for a SGWB signal in (simulated) data. Although we use simulated noise and SGWB signals for making these comparisons, our method can be straightforwardly applied on real data.
C1 [Talukder, Dipongkar; Bose, Sukanta] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA.
[Mitra, Sanjit] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mitra, Sanjit] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Mitra, Sanjit] Observ Cote Azur, F-06304 Nice 4, France.
RP Talukder, D (reprint author), Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA.
EM talukder_d@wsu.edu; smitra@ligo.caltech.edu; sukanta@wsu.edu
OI Talukder, Dipongkar/0000-0002-9178-8870
FU Centre National d'Etudes Spatiales (France); National Science Foundation
[PHY-0855679, PHY-0757058]; National Aeronautics and Space
Administration
FX We thank Joe Romano, Stefan Ballmer, and Warren Anderson for
discussions, careful reading of the manuscript, and helpful comments. We
would also like to thank Bruce Allen, Sanjeev Dhurandhar, Albert
Lazzarini, Vuk Mandic, Himan Mukhopadhyay, Alan Weinstein, and Holger
Pletsch for helpful discussions. S. M. would like to acknowledge the
Centre National d'Etudes Spatiales (France) for supporting part of the
research. This work was supported in part by NSF Grant No. PHY-0855679.
Part of the research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. LIGO
was constructed by the California Institute of Technology and
Massachusetts Institute of Technology with funding from the National
Science Foundation and operates under cooperative agreement PHY-0757058.
NR 30
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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 MAR 4
PY 2011
VL 83
IS 6
AR 063002
DI 10.1103/PhysRevD.83.063002
PG 16
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 730BX
UT WOS:000288006000002
ER
PT J
AU Rignot, E
Velicogna, I
van den Broeke, MR
Monaghan, A
Lenaerts, J
AF Rignot, E.
Velicogna, I.
van den Broeke, M. R.
Monaghan, A.
Lenaerts, J.
TI Acceleration of the contribution of the Greenland and Antarctic ice
sheets to sea level rise
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MASS-LOSS; JAKOBSHAVN ISBRAE; GLACIERS; VELOCITY; SNOWFALL; RETREAT;
BALANCE
AB Ice sheet mass balance estimates have improved substantially in recent years using a variety of techniques, over different time periods, and at various levels of spatial detail. Considerable disparity remains between these estimates due to the inherent uncertainties of each method, the lack of detailed comparison between independent estimates, and the effect of temporal modulations in ice sheet surface mass balance. Here, we present a consistent record of mass balance for the Greenland and Antarctic ice sheets over the past two decades, validated by the comparison of two independent techniques over the last 8 years: one differencing perimeter loss from net accumulation, and one using a dense time series of time-variable gravity. We find excellent agreement between the two techniques for absolute mass loss and acceleration of mass loss. In 2006, the Greenland and Antarctic ice sheets experienced a combined mass loss of 475 +/- 158 Gt/yr, equivalent to 1.3 +/- 0.4 mm/yr sea level rise. Notably, the acceleration in ice sheet loss over the last 18 years was 21.9 +/- 1 Gt/yr(2) for Greenland and 14.5 +/- 2 Gt/yr(2) for Antarctica, for a combined total of 36.3 +/- 2 Gt/yr(2). This acceleration is 3 times larger than for mountain glaciers and ice caps (12 +/- 6 Gt/yr(2)). If this trend continues, ice sheets will be the dominant contributor to sea level rise in the 21st century. Citation: Rignot, E., I. Velicogna, M. R. van den Broeke, A. Monaghan, and J. Lenaerts (2011), Acceleration of the contribution of the Greenland and Antarctic ice sheets to sea level rise, Geophys. Res. Lett., 38, L05503, doi:10.1029/2011GL046583.
C1 [Rignot, E.; Velicogna, I.] Univ Calif Irvine, Irvine, CA 92697 USA.
[Rignot, E.; Velicogna, I.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[van den Broeke, M. R.; Lenaerts, J.] Univ Utrecht, Inst Marine & Atmospher Res, NL-3584 CC Utrecht, Netherlands.
[Monaghan, A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Rignot, E (reprint author), Univ Calif Irvine, 226 Croul Hall, Irvine, CA 92697 USA.
EM erignot@uci.edu
RI Van den Broeke, Michiel/F-7867-2011; Rignot, Eric/A-4560-2014; Lenaerts,
Jan/D-9423-2012;
OI Van den Broeke, Michiel/0000-0003-4662-7565; Rignot,
Eric/0000-0002-3366-0481; Lenaerts, Jan/0000-0003-4309-4011; Monaghan,
Andrew/0000-0002-8170-2359
FU National Aeronautics and Space Administration; National Science
Foundation; Utrecht University; Netherlands Polar Programme
FX This work was performed at the Earth System Science Department of
Physical Sciences, University of California Irvine and at the California
Institute of Technology's Jet Propulsion Laboratory under a contract
with the National Aeronautics and Space Administration's Cryospheric
Science Program. NCAR is funded by the National Science Foundation. This
work was financially supported by Utrecht University and the Netherlands
Polar Programme.
NR 30
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U1 34
U2 221
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 MAR 4
PY 2011
VL 38
AR L05503
DI 10.1029/2011GL046583
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 731DR
UT WOS:000288087000005
ER
PT J
AU Hakkinen, S
Rhines, PB
Worthen, DL
AF Haekkinen, Sirpa
Rhines, Peter B.
Worthen, Denise L.
TI Warm and saline events embedded in the meridional circulation of the
northern North Atlantic
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID THERMOHALINE CIRCULATION; SUBPOLAR GYRE; OCEAN; REANALYSIS; WATER;
OSCILLATION; VARIABILITY; TRANSPORT
AB Ocean state estimates from 1958 to 2005 from the Simple Ocean Assimilation System (SODA) system are analyzed to understand circulation between subtropical and subpolar Atlantic and their connection with atmospheric forcing. This analysis shows three periods (1960s, around 1980, and 2000s) with enhanced warm, saline waters reaching high latitudes, alternating with freshwater events originating at high latitudes. It complements surface drifter and altimetry data showing the subtropical-subpolar exchange leading to a significant temperature and salinity increase in the northeast Atlantic after 2001. The warm water limb of the Atlantic meridional overturning cell represented by SODA expanded in density/salinity space during these warm events. Tracer simulations using SODA velocities also show decadal variation of the Gulf Stream waters reaching the subpolar gyre and Nordic seas. The negative phase of the North Atlantic Oscillation index, usually invoked in such variability, fails to predict the warming and salinization in the early 2000s, with salinities not seen since the 1960s. Wind stress curl variability provided a linkage to this subtropical/subpolar gyre exchange as illustrated using an idealized two-layer circulation model. The ocean response to the modulation of the climatological wind stress curl pattern was found to be such that the northward penetration of subtropical tracers is enhanced when amplitude of the wind stress curl is weaker than normal. In this case both the subtropical and subpolar gyres weaken and the subpolar density surfaces relax; hence, the polar front moves westward, opening an enhanced northward access of the subtropical waters in the eastern boundary current.
C1 [Haekkinen, Sirpa; Worthen, Denise L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rhines, Peter B.] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA.
[Worthen, Denise L.] Wyle ITS, Greenbelt, MD USA.
RP Hakkinen, S (reprint author), NASA, Goddard Space Flight Ctr, Code 614-1, Greenbelt, MD 20771 USA.
EM sirpa.m.hakkinen@nasa.gov
RI Hakkinen, Sirpa/E-1461-2012
FU NASA through the OSTM Science Team
FX We sincerely thank both of our referees for constructive criticism and
helpful comments to improve the manuscript. S.H. and D.L.W. gratefully
acknowledge the support from NASA Headquarters Physical Oceanography
Program and OSTM Science Team for this work. P.B.R. is supported by NASA
through the OSTM Science Team.
NR 28
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U1 2
U2 26
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 MAR 4
PY 2011
VL 116
AR C03006
DI 10.1029/2010JC006275
PG 13
WC Oceanography
SC Oceanography
GA 731ER
UT WOS:000288089600002
ER
PT J
AU Simon, JI
Hutcheon, ID
Simon, SB
Matzel, JEP
Ramon, EC
Weber, PK
Grossman, L
DePaolo, DJ
AF Simon, Justin I.
Hutcheon, Ian D.
Simon, Steven B.
Matzel, Jennifer E. P.
Ramon, Erick C.
Weber, Peter K.
Grossman, Lawrence
DePaolo, Donald J.
TI Oxygen Isotope Variations at the Margin of a CAI Records Circulation
Within the Solar Nebula
SO SCIENCE
LA English
DT Article
ID SHOCK-WAVE MODEL; REFRACTORY INCLUSIONS; CARBONACEOUS CHONDRITES;
PROTOPLANETARY NEBULA; RICH INCLUSIONS; CHONDRULE; ALLENDE; DISKS;
TRANSPORT; COMPONENT
AB Micrometer-scale analyses of a calcium-, aluminum-rich inclusion (CAI) and the characteristic mineral bands mantling the CAI reveal that the outer parts of this primitive object have a large range of oxygen isotope compositions. The variations are systematic; the relative abundance of O-16 first decreases toward the CAI margin, approaching a planetary-like isotopic composition, then shifts to extremely O-16-rich compositions through the surrounding rim. The variability implies that CAIs probably formed from several oxygen reservoirs. The observations support early and short-lived fluctuations of the environment in which CAIs formed, either because of transport of the CAIs themselves to distinct regions of the solar nebula or because of varying gas composition near the proto-Sun.
C1 [Simon, Justin I.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off KR111, Houston, TX 77058 USA.
[Simon, Justin I.; DePaolo, Donald J.] Univ Calif Berkeley, Ctr Isotope Geochem, Berkeley, CA 94720 USA.
[Hutcheon, Ian D.; Matzel, Jennifer E. P.; Ramon, Erick C.; Weber, Peter K.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
[Simon, Steven B.; Grossman, Lawrence] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
RP Simon, JI (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res Off KR111, Houston, TX 77058 USA.
EM justin.i.simon@nasa.gov
RI Simon, Justin/D-7015-2011
FU Institute of Geophysics and Planetary Physics at LLNL; NASA; U.S.
Department of Energy at LLNL [DE-AC52-07NA27344]
FX This work was supported by grants from the Institute of Geophysics and
Planetary Physics at LLNL (J.I.S. and D.J.D.), the NASA Origins program
(I.D.H., J.E.P.M., and J.I.S.), and the NASA Cosmochemistry program
(L.G. and I.D.H.). Work was performed under the auspices of the U.S.
Department of Energy at LLNL under contract DE-AC52-07NA27344.
NR 27
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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 MAR 4
PY 2011
VL 331
IS 6021
BP 1175
EP 1178
DI 10.1126/science.1197970
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 729SN
UT WOS:000287971200037
PM 21385711
ER
PT J
AU Zhou, XY
Sun, W
Ridley, AJ
Mende, SB
AF Zhou, X. -Y.
Sun, W.
Ridley, A. J.
Mende, S. B.
TI Joule heating associated with auroral electrojets during magnetospheric
substorms
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID IONOSPHERIC ELECTRIC-FIELDS; POLAR-CAP INDEX; PRECIPITATION POWER;
MAGNETOTAIL ENERGY; ALIGNED CURRENTS; EMPIRICAL-MODEL; CURRENT SYSTEMS;
SOLAR-WIND; CONDUCTANCES; PARAMETERS
AB The magnetospheric substorm is important not only because it involves many interesting physical processes but also because it plays a key role in the solar wind energy dissipation into the ionosphere. This paper focuses on a quantitative description of the Joule heating production rate generated during substorms by auroral electrojets that are composed of two aspects: convection electrojets and the substorm electrojet. First, the natural orthogonal component (NOC) method is carefully discussed by examining its methodology and by comparing with other mathematical techniques and ionospheric observations. It is concluded that the NOC method is a very helpful and unique method that sheds insight into the electric potential patterns in the high-latitude ionosphere. Then, using the AMIE electric potential and the NOC method, the sawtooth event on 18 April 2002 and an isolated substorm on 15 November 2001 are studied. Electric fields and Joule heating rates corresponding to the convection electrojets and the substorm electrojet, respectively, are obtained. It is found that the Joule heating associated with the substorm electrojet is only one fourth to one third of that associated with the convection electrojets during the sawtooth event. However, the former dominated the total Joule heating during the expansion phase of the isolated substorm, and the two types of the Joule heating are comparable in magnitude in the isolated substorm recovery phase.
C1 [Zhou, X. -Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sun, W.] Univ Alaska, Inst Geophys, Fairbanks, AK 99775 USA.
[Ridley, A. J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Mende, S. B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Zhou, XY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA.
EM xiaoyan.zhou@jpl.nasa.gov
RI Ridley, Aaron/F-3943-2011
OI Ridley, Aaron/0000-0001-6933-8534
FU NSF [ATM-0639336]; AFOSR [FA9550-070434]
FX The results reported here represent one aspect of research carried out
by the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
Research at the University of Michigan was supported by NSF grant
ATM-0639336 and by AFOSR grant FA9550-070434.
NR 43
TC 2
Z9 2
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR 3
PY 2011
VL 116
AR A00I28
DI 10.1029/2010JA015804
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 731CR
UT WOS:000288084400001
ER
PT J
AU Butchart, N
Charlton-Perez, AJ
Cionni, I
Hardiman, SC
Haynes, PH
Kruger, K
Kushner, PJ
Newman, PA
Osprey, SM
Perlwitz, J
Sigmond, M
Wang, L
Akiyoshi, H
Austin, J
Bekki, S
Baumgaertner, A
Braesicke, P
Bruhl, C
Chipperfield, M
Dameris, M
Dhomse, S
Eyring, V
Garcia, R
Garny, H
Jockel, P
Lamarque, JF
Marchand, M
Michou, M
Morgenstern, O
Nakamura, T
Pawson, S
Plummer, D
Pyle, J
Rozanov, E
Scinocca, J
Shepherd, TG
Shibata, K
Smale, D
Teyssedre, H
Tian, W
Waugh, D
Yamashita, Y
AF Butchart, N.
Charlton-Perez, A. J.
Cionni, I.
Hardiman, S. C.
Haynes, P. H.
Krueger, K.
Kushner, P. J.
Newman, P. A.
Osprey, S. M.
Perlwitz, J.
Sigmond, M.
Wang, L.
Akiyoshi, H.
Austin, J.
Bekki, S.
Baumgaertner, A.
Braesicke, P.
Bruehl, C.
Chipperfield, M.
Dameris, M.
Dhomse, S.
Eyring, V.
Garcia, R.
Garny, H.
Joeckel, P.
Lamarque, J-F
Marchand, M.
Michou, M.
Morgenstern, O.
Nakamura, T.
Pawson, S.
Plummer, D.
Pyle, J.
Rozanov, E.
Scinocca, J.
Shepherd, T. G.
Shibata, K.
Smale, D.
Teyssedre, H.
Tian, W.
Waugh, D.
Yamashita, Y.
TI Multimodel climate and variability of the stratosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID QUANTITATIVE PERFORMANCE METRICS; MIDDLE-ATMOSPHERE CLIMATOLOGIES;
VERTICALLY EXTENDED VERSION; FINAL WARMING EVENTS; PART I;
METEOROLOGICAL ANALYSES; TRANSIENT SIMULATION; ARCTIC STRATOSPHERE;
SUDDEN WARMINGS; TECHNICAL NOTE
AB The stratospheric climate and variability from simulations of sixteen chemistry-climate models is evaluated. On average the polar night jet is well reproduced though its variability is less well reproduced with a large spread between models. Polar temperature biases are less than 5 K except in the Southern Hemisphere (SH) lower stratosphere in spring. The accumulated area of low temperatures responsible for polar stratospheric cloud formation is accurately reproduced for the Antarctic but underestimated for the Arctic. The shape and position of the polar vortex is well simulated, as is the tropical upwelling in the lower stratosphere. There is a wide model spread in the frequency of major sudden stratospheric warnings (SSWs), late biases in the breakup of the SH vortex, and a weak annual cycle in the zonal wind in the tropical upper stratosphere. Quantitatively, "metrics" indicate a wide spread in model performance for most diagnostics with systematic biases in many, and poorer performance in the SH than in the Northern Hemisphere (NH). Correlations were found in the SH between errors in the final warming, polar temperatures, the leading mode of variability, and jet strength, and in the NH between errors in polar temperatures, frequency of major SSWs, and jet strength. Models with a stronger QBO have stronger tropical upwelling and a colder NH vortex. Both the qualitative and quantitative analysis indicate a number of common and long-standing model problems, particularly related to the simulation of the SH and stratospheric variability.
C1 [Butchart, N.; Hardiman, S. C.] Met Off Hadley Ctr, Exeter EX1 3PB, Devon, England.
[Charlton-Perez, A. J.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
[Cionni, I.; Dameris, M.; Eyring, V.; Garny, H.] Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atmosphare, D-82234 Oberpfaffenhofen, Germany.
[Haynes, P. H.; Braesicke, P.; Pyle, J.] Univ Cambridge, Natl Ctr Atmospher Sci, Cambridge CB2 1SZ, England.
[Krueger, K.] Univ Kiel, Leibniz Inst Marine Sci, IFM GEOMAR, D-24148 Kiel, Germany.
[Kushner, P. J.; Sigmond, M.; Wang, L.; Shepherd, T. G.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A1, Canada.
[Newman, P. A.; Pawson, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Osprey, S. M.] Univ Oxford, Dept Phys, Natl Ctr Atmospher Sci, Oxford OX1 2JD, England.
[Perlwitz, J.] Univ Colorado, Cooperat Inst Res Environm Sci, Div Phys Sci, Boulder, CO 80309 USA.
[Perlwitz, J.] NOAA, Earth Syst Res Lab, Boulder, CO 80309 USA.
[Akiyoshi, H.; Nakamura, T.; Yamashita, Y.] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
[Austin, J.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Bekki, S.; Marchand, M.] Univ Paris 06, Inst Pierre Simon Laplace, LATMOS, F-75252 Paris 05, France.
[Baumgaertner, A.; Bruehl, C.; Garny, H.; Joeckel, P.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Chipperfield, M.; Dhomse, S.; Tian, W.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Garcia, R.; Lamarque, J-F] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Michou, M.] Meteo France, CNRS, GAME CNRM, F-31057 Toulouse 01, France.
[Morgenstern, O.; Smale, D.] Natl Inst Water & Atmospher Res, Lauder, New Zealand.
[Plummer, D.] Environm Canada, Toronto, ON M3H 5T4, Canada.
[Rozanov, E.] World Radiat Ctr, Phys Meteorol Observ, CH-7260 Davos, Switzerland.
[Scinocca, J.] Univ Victoria, Meteorol Serv Canada, Victoria, BC V8W 2Y2, Canada.
[Shibata, K.] Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan.
[Waugh, D.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
RP Butchart, N (reprint author), Met Off Hadley Ctr, FitzRoy Rd, Exeter EX1 3PB, Devon, England.
EM neal.butchart@metoffice.gov.uk; a.j.charlton@reading.ac.uk
RI Braesicke, Peter/D-8330-2016; Kushner, Paul/H-6716-2016; Pawson,
Steven/I-1865-2014; Eyring, Veronika/O-9999-2016; Osprey,
Scott/P-6621-2016; Lamarque, Jean-Francois/L-2313-2014; Perlwitz,
Judith/B-7201-2008; Wang, Lei/F-1269-2015; bekki, slimane/J-7221-2015;
Nakamura, Tetsu/M-7914-2015; Jockel, Patrick/C-3687-2009; Dhomse,
Sandip/C-8198-2011; Rozanov, Eugene/A-9857-2012; Charlton-Perez,
Andrew/F-4079-2010; Newman, Paul/D-6208-2012; Sigmond, Michael
/K-3169-2012; Baumgaertner, Andreas/C-4830-2011; Chipperfield,
Martyn/H-6359-2013;
OI Braesicke, Peter/0000-0003-1423-0619; Kushner, Paul/0000-0002-6404-4518;
Pawson, Steven/0000-0003-0200-717X; Eyring,
Veronika/0000-0002-6887-4885; Osprey, Scott/0000-0002-8751-1211;
Lamarque, Jean-Francois/0000-0002-4225-5074; Perlwitz,
Judith/0000-0003-4061-2442; Wang, Lei/0000-0002-1618-1796; bekki,
slimane/0000-0002-5538-0800; Nakamura, Tetsu/0000-0002-2056-7392;
Jockel, Patrick/0000-0002-8964-1394; Dhomse, Sandip/0000-0003-3854-5383;
Rozanov, Eugene/0000-0003-0479-4488; Charlton-Perez,
Andrew/0000-0001-8179-6220; Newman, Paul/0000-0003-1139-2508; Sigmond,
Michael /0000-0003-2191-9756; Baumgaertner, Andreas/0000-0002-4740-0701;
Chipperfield, Martyn/0000-0002-6803-4149; Morgenstern,
Olaf/0000-0002-9967-9740; Haynes, Peter/0000-0002-7726-6988
FU Joint DECC/Defra Met Office Hadley Centre [GA01101]; Ministry of the
Environment of Japan [A-071, A-0903]; European Commission
FX We acknowledge the Chemistry-Climate Model Validation Activity (CCMVal)
of the World Climate Research Programme's (WCRP) Stratospheric Processes
and their Role in Climate (SPARC) project for organizing and
coordinating the model data analysis, and the British Atmospheric Data
Centre (BADC) for collecting and archiving the CCMVal model output.
ECMWF ERA-Interim data used in this study have been provided by ECMWF.
The contribution from Neal Butchart and Steven Hardiman was supported by
the Joint DECC/Defra Met Office Hadley Centre Climate Programme
(GA01101). The ERA-Interim results shown in Figure 10 were kindly
provided by William Seviour of the University of Cambridge. CCSRNIES
research was supported by the Global Environmental Research Fund of the
Ministry of the Environment of Japan (A-071 and A-0903) and the
simulations were completed with the super computer at CGER, NIES. The
MRI simulation was made with the supercomputer at the National Institute
for Environmental Studies, Japan. The contribution from the LATMOS-IPSL
was supported by the European Commission through the funding of the
RECONCILE and GEOMON projects.
NR 72
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U1 3
U2 58
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 MAR 3
PY 2011
VL 116
AR D05102
DI 10.1029/2010JD014995
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 731DX
UT WOS:000288087600001
ER
PT J
AU Fuller, T
Thomassen, HA
Mulembakani, PM
Johnston, SC
Lloyd-Smith, JO
Kisalu, NK
Lutete, TK
Blumberg, S
Fair, JN
Wolfe, ND
Shongo, RL
Formenty, P
Meyer, H
Wright, LL
Muyembe, JJ
Buermann, W
Saatchi, SS
Okitolonda, E
Hensley, L
Smith, TB
Rimoin, AW
AF Fuller, Trevon
Thomassen, Henri A.
Mulembakani, Prime M.
Johnston, Sara C.
Lloyd-Smith, James O.
Kisalu, Neville K.
Lutete, Timothee K.
Blumberg, Seth
Fair, Joseph N.
Wolfe, Nathan D.
Shongo, Robert L.
Formenty, Pierre
Meyer, Hermann
Wright, Linda L.
Muyembe, Jean-Jacques
Buermann, Wolfgang
Saatchi, Sassan S.
Okitolonda, Emile
Hensley, Lisa
Smith, Thomas B.
Rimoin, Anne W.
TI Using Remote Sensing to Map the Risk of Human Monkeypox Virus in the
Congo Basin
SO ECOHEALTH
LA English
DT Article
DE monkeypox; orthopoxvirus; smallpox vaccination; epidemiology; active
surveillance; human transmission
ID ECOLOGICAL NICHE; SPECIES DISTRIBUTIONS; DISTRIBUTION MODELS;
TRANSMISSION; POPULATION; AFRICA; MAXENT; ZAIRE
AB Although the incidence of human monkeypox has greatly increased in Central Africa over the last decade, resources for surveillance remain extremely limited. We conducted a geospatial analysis using existing data to better inform future surveillance efforts. Using active surveillance data collected between 2005 and 2007, we identified locations in Sankuru district, Democratic Republic of Congo (DRC) where there have been one or more cases of human monkeypox. To assess what taxa constitute the main reservoirs of monkeypox, we tested whether human cases were associated with (i) rope squirrels (Funisciurus sp.), which were implicated in monkeypox outbreaks elsewhere in the DRC in the 1980s, or (ii) terrestrial rodents in the genera Cricetomys and Graphiurus, which are believed to be monkeypox reservoirs in West Africa. Results suggest that the best predictors of human monkeypox cases are proximity to dense forests and associated habitat preferred by rope squirrels. The risk of contracting monkeypox is significantly greater near sites predicted to be habitable for squirrels (OR = 1.32; 95% CI 1.08-1.63). We recommend that semi-deciduous rainforests with oil-palm, the rope squirrel's main food source, be prioritized for monitoring.
C1 [Lloyd-Smith, James O.; Blumberg, Seth; Rimoin, Anne W.] NIH, Fogarty Int Ctr, Bethesda, MD 20892 USA.
[Fuller, Trevon; Thomassen, Henri A.; Buermann, Wolfgang; Saatchi, Sassan S.; Smith, Thomas B.] Univ Calif Los Angeles, Inst Environm, Ctr Trop Res, Los Angeles, CA 90095 USA.
[Mulembakani, Prime M.; Lutete, Timothee K.; Okitolonda, Emile] Kinshasa Sch Publ Hlth, Kinshasa, Zaire.
[Johnston, Sara C.; Hensley, Lisa] USA, Med Res Inst Infect Dis, Frederick, MD USA.
[Lloyd-Smith, James O.; Blumberg, Seth; Smith, Thomas B.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA.
[Kisalu, Neville K.] Univ Calif Los Angeles, Dept Microbiol, Los Angeles, CA 90024 USA.
[Fair, Joseph N.; Wolfe, Nathan D.] Global Viral Forecasting Initiat, San Francisco, CA USA.
[Shongo, Robert L.] Minist Hlth, Kinshasa, Zaire.
[Formenty, Pierre] WHO, Dept Global Alert & Response, CH-1211 Geneva, Switzerland.
[Meyer, Hermann] Bundeswehr Inst Microbiol, Munich, Germany.
[Wright, Linda L.] Eunice Kennedy Shriver Natl Inst Child Hlth & Hum, Bethesda, MD USA.
[Muyembe, Jean-Jacques] Natl Inst Biomed Res, Kinshasa, Zaire.
[Buermann, Wolfgang] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, Radar Sci Tech Grp, Pasadena, CA USA.
[Rimoin, Anne W.] Univ Calif Los Angeles, Sch Publ Hlth, Dept Epidemiol, Los Angeles, CA 90095 USA.
RP Rimoin, AW (reprint author), NIH, Fogarty Int Ctr, Bldg 10, Bethesda, MD 20892 USA.
EM arimoin@ucla.edu
RI Lloyd-Smith, James/K-4080-2012; Valle, Ruben/A-7512-2013
OI Lloyd-Smith, James/0000-0001-7941-502X;
FU Faucett Family Foundation; National Institutes of Health, National
Institute of Child Health and Human Development, Bethesda, MD, USA;
National Science Foundation-National Institutes of Health [EF-0430146];
RAPIDD of the Science and Technology Directorate, Department of Homeland
Security; Fogarty International Center, National Institutes of Health;
National Institute of Allergy and Infectious Diseases
[EID-1R01AI074059-01]
FX This work was made possible by the generous support of the Faucett
Family Foundation. We respectfully thank the DRC Ministry of Health and
local health workers who were responsible for specimen collection and
case investigation. Additional support for this study was provided by
the National Institutes of Health, National Institute of Child Health
and Human Development, Bethesda, MD, USA, by the joint National Science
Foundation-National Institutes of Health Ecology of Infectious Diseases
Program (grant number EF-0430146), by the RAPIDD program of the Science
and Technology Directorate, Department of Homeland Security, by the
Fogarty International Center, National Institutes of Health, and by the
National Institute of Allergy and Infectious Diseases (grant number
EID-1R01AI074059-01). We thank two anonymous reviewers for comments that
improved the manuscript.
NR 40
TC 14
Z9 15
U1 1
U2 15
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1612-9202
J9 ECOHEALTH
JI EcoHealth
PD MAR
PY 2011
VL 8
IS 1
BP 14
EP 25
DI 10.1007/s10393-010-0355-5
PG 12
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 862PI
UT WOS:000298105300002
PM 21069425
ER
PT J
AU Graham, SM
Adler, MA
AF Graham, Stephen M.
Adler, Matthew A.
TI Determining the Slope and Quality of Fit for the Linear Part of a Test
Record
SO JOURNAL OF TESTING AND EVALUATION
LA English
DT Article
DE linear regression; mechanical testing; analysis of residuals
AB It is often necessary to determine the slope of a linear region within a test record, and for standardization purposes, it is desirable to have a method for determining the slope that is not subjective. A fully automated algorithm is presented, which is independent of operator judgment for data sets that meet specific quality of data and fit criteria. The algorithm uses analysis of residuals to simulate the visual process of determining the linear region. Analysis of benchmark and real test data provide validation that the algorithm correctly differentiates between problem data (noisy, insufficient digital resolution, or no significant linear range) and good data.
C1 [Graham, Stephen M.] USN Acad, Dept Mech Engn, Annapolis, MD 21402 USA.
[Adler, Matthew A.] NASA, George C Marshall Space Flight Ctr, Jacobs ESTS Grp, ICRC, Huntsville, AL 35812 USA.
RP Graham, SM (reprint author), USN Acad, Dept Mech Engn, Annapolis, MD 21402 USA.
EM smgraham@usna.edu; matthew.a.adler@nasa.gov
NR 5
TC 4
Z9 4
U1 0
U2 4
PU AMER SOC TESTING MATERIALS
PI W CONSHOHOCKEN
PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 USA
SN 0090-3973
EI 1945-7553
J9 J TEST EVAL
JI J. Test. Eval.
PD MAR
PY 2011
VL 39
IS 2
BP 260
EP 268
DI 10.1520/JTE103038
PG 9
WC Materials Science, Characterization & Testing
SC Materials Science
GA 842JT
UT WOS:000296596200018
ER
PT J
AU Schmidt, GA
Mann, ME
Rutherford, SD
AF Schmidt, Gavin A.
Mann, Michael E.
Rutherford, Scott D.
TI DISCUSSION OF: A STATISTICAL ANALYSIS OF MULTIPLE TEMPERATURE PROXIES:
ARE RECONSTRUCTIONS OF SURFACE TEMPERATURES OVER THE LAST 1000 YEARS
RELIABLE?
SO ANNALS OF APPLIED STATISTICS
LA English
DT Editorial Material
C1 [Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Mann, Michael E.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Mann, Michael E.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA.
[Rutherford, Scott D.] Roger Williams Univ, Dept Environm Sci, Bristol, RI 02809 USA.
RP Schmidt, GA (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM Gavin.A.Schmidt@nasa.gov; mann@psu.edu
RI Schmidt, Gavin/D-4427-2012; Mann, Michael/B-8472-2017
OI Schmidt, Gavin/0000-0002-2258-0486; Mann, Michael/0000-0003-3067-296X
NR 11
TC 4
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U1 0
U2 2
PU INST MATHEMATICAL STATISTICS
PI CLEVELAND
PA 3163 SOMERSET DR, CLEVELAND, OH 44122 USA
SN 1932-6157
J9 ANN APPL STAT
JI Ann. Appl. Stat.
PD MAR
PY 2011
VL 5
IS 1
BP 65
EP 70
DI 10.1214/10-AOAS398D
PG 6
WC Statistics & Probability
SC Mathematics
GA 827TQ
UT WOS:000295451800008
ER
PT J
AU Gormly, S
Herron, J
Flynn, M
Hammoudeh, M
Shaw, H
AF Gormly, Sherwin
Herron, Jack
Flynn, Michael
Hammoudeh, Mona
Shaw, Hali
TI Forward osmosis for applications in sustainable energy development
SO DESALINATION AND WATER TREATMENT
LA English
DT Article
DE Forward osmosis; Pressure retarded osmosis; Osmotic power; Osmotic
wastewater; treatment; Water/power nexus
ID PRESSURE-RETARDED OSMOSIS; EQUATION
AB Forward osmosis (FO) provides a method of harvesting the osmotic potential difference between fresh and saline waters to produce electricity. FO occurs when fresh water and saline water are placed on opposide sides of a semi-permeable membrane. When this occurs water naturally flows from the freshwater side of the membrane to the saline side. This water flux continues until the osmotic pressure difference on both sides of the membrane equalize. The water flux will cause the pressure to increase in the saline water. If the saline water is seawater the pressure can reach as high as 410 psi. This pressure can be harvested as hydraulic power, similar to that of a hydroelectric dam. Such a system is called pressure retarded forward osmosis (PRO) and it can be used anywhere fresh water mixes with oceans, is reported to be in excess of 1600 tera-watt-hour (TWH) per year [1]. In arid regions, such as California, where few major rivers reach the ocean, the applicability of PRO is limited. In these regions it makes sense to look for alternative sources of fresh water. This project evaluates an approach where, rather than siteing a PRO power plant in ways that potentially impact sensitive costal environments, they are sited at wastewater treatment plants that discharge into the ocean or other sources of saline water and are effective in a comprehensive environmental management and design role. Electricity can then be generated from the mixing of the treatment plants outfall and seawater while providing a high level of additional treatment and environmental protection. In the state of California alone, 1,350 million gallons per day of treated municipal wastewater is discharged into the Pacific Ocean. Using PRO this represnets about a 26 megawatt resource. In addition to the electricity produced, the PRO also provides tertiary treatment of the wastewater treatment plant's outfall. It is comparable to treatment with reverse osmosis membranes. The combination of PRO and tertiary treatment (PRO/TT) provides the mutual benefit of sustainable power production and advanced wastewater treatment. This is particularly important in locations where regulation is requiring treatment plants to tertiary treat wastewater. PRO/TT can be used to offset the cost of providing treatment by generating electricity that can be sold for profit or used to help power the treatment plant.
C1 [Gormly, Sherwin; Herron, Jack] Hydrat Technol Innovat, Albany, OR 97322 USA.
[Flynn, Michael] NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94035 USA.
[Hammoudeh, Mona; Shaw, Hali] Univ Space Res Assoc, Moffett Field, CA USA.
RP Gormly, S (reprint author), Hydrat Technol Innovat, 2484 Ferry St SW, Albany, OR 97322 USA.
EM sherwingormly@gmail.com; michael.flynn@nasa.gov
NR 11
TC 7
Z9 7
U1 14
U2 49
PU DESALINATION PUBL
PI HOPKINTON
PA 36 WALCOTT VALLEY DRIVE,, HOPKINTON, MA 01748 USA
SN 1944-3994
J9 DESALIN WATER TREAT
JI Desalin. Water Treat.
PD MAR
PY 2011
VL 27
IS 1-3
BP 327
EP 333
DI 10.5004/dwt.2011.2596
PG 7
WC Engineering, Chemical; Water Resources
SC Engineering; Water Resources
GA 805RF
UT WOS:000293746000046
ER
PT J
AU Jezek, KC
Gogineni, S
Wu, X
Rodriguez, E
Rodriguez-Morales, F
Hoch, A
Freeman, A
Sonntag, JG
AF Jezek, Kenneth C.
Gogineni, Sivaprasad
Wu, X.
Rodriguez, E.
Rodriguez-Morales, Fernando
Hoch, A.
Freeman, Anthony
Sonntag, John G.
TI Two-Frequency Radar Experiments for Sounding Glacier Ice and Mapping the
Topography of the Glacier Bed
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Airborne radar; arctic; geoscience; radar clutter
ID GREENLAND
AB We performed airborne experiments using 150- and 450-MHz radars to measure ice thickness on the Greenland ice sheet. Our objectives were to investigate to what degree surface clutter obscures the basal echo when airborne measurements are made at different elevations and at different frequencies. We also explored interferometric techniques for processing the data to form swath measurements of ice thickness. We found that surface clutter was minimal for either frequency when operated at low aircraft elevations (500 m above the ice sheet surface) or over benign regions of the ice sheet. Because signal-to-clutter ratios were favorable, we found that we could retrieve the swath measurements of ice thickness at both frequencies using an interferometric technique. At high elevation, surface clutter degraded the 150-MHz signal, but the nadir ice thickness was still retrievable. The basal return in high-elevation 450-MHz data was detectable only after additional beam-steering techniques were applied to the data to reduce the surface clutter signal. Results suggest that interferometric cross-track ice-thickness measurements can be successfully made given a sufficient number of antenna elements driven at either 150 or 450 MHz and flown at both high and low elevations over the interior ice sheet.
C1 [Jezek, Kenneth C.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Gogineni, Sivaprasad; Rodriguez-Morales, Fernando; Hoch, A.] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
[Wu, X.; Rodriguez, E.; Freeman, Anthony] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sonntag, John G.] URS Corp, San Francisco, CA USA.
[Sonntag, John G.] NASA, Wallops Isl, VA 23337 USA.
RP Jezek, KC (reprint author), Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
FU NASA Earth Science and Technology Office; Office of Polar Programs of
the National Science Foundation
FX Manuscript received May 14, 2010; revised July 6, 2010; accepted August
5, 2010. Date of publication October 14, 2010; date of current version
February 25, 2011. This work was supported in part by the NASA Earth
Science and Technology Office and in part by the Office of Polar
Programs of the National Science Foundation.
NR 16
TC 12
Z9 12
U1 0
U2 3
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 MAR
PY 2011
VL 49
IS 3
BP 920
EP 929
DI 10.1109/TGRS.2010.2071387
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 725PN
UT WOS:000287658000003
ER
PT J
AU Bertacca, D
Raccanelli, A
Piattella, OF
Pietrobon, D
Bartolo, N
Matarrese, S
Giannantonio, T
AF Bertacca, Daniele
Raccanelli, Alvise
Piattella, Oliver F.
Pietrobon, Davide
Bartolo, Nicola
Matarrese, Sabino
Giannantonio, Tommaso
TI CMB-galaxy correlation in Unified Dark Matter scalar field cosmologies
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE dark matter theory; integrated Sachs-Wolfe effect; dark energy theory;
galaxy surveys
ID ANISOTROPY-PROBE OBSERVATIONS; DIGITAL SKY SURVEY; ENERGY CONSTRAINTS;
CROSS-CORRELATION; CHAPLYGIN-GAS; IA SUPERNOVAE; RADIO-SOURCES; LIGHT
CURVES; MICROWAVE; CONSTANT
AB We present an analysis of the cross-correlation between the CMB and the large-scale structure (LSS) of the Universe in Unified Dark Matter (UDM) scalar field cosmologies. We work out the predicted cross-correlation function in UDM models, which depends on the speed of sound of the unified component, and compare it with observations from six galaxy catalogues (NVSS, HEAO, 2MASS, and SDSS main galaxies, luminous red galaxies, and quasars). We sample the value of the speed of sound and perform a likelihood analysis, finding that the UDM model is as likely as the Lambda CDM, and is compatible with observations for a range of values of c(proportional to) (the value of the sound speed at late times) on which structure formation depends. In particular, we obtain an upper bound of c(proportional to)(2) <= 0.009 at 95% confidence level, meaning that the Lambda CDM model, for which c(proportional to)(2) = 0, is a good fit to the data, while the posterior probability distribution peaks at the value c(proportional to)(2) = 10(-4). Finally, we study the time dependence of the deviation from Lambda CDM via a tomographic analysis using a mock redshift distribution and we find that the largest deviation is for low-redshift sources, suggesting that future low-z surveys will be best suited to constrain UDM models.
C1 [Bertacca, Daniele; Bartolo, Nicola; Matarrese, Sabino] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bertacca, Daniele; Bartolo, Nicola; Matarrese, Sabino] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bertacca, Daniele; Raccanelli, Alvise] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Piattella, Oliver F.] Univ Fed Espirito Santo, Dept Fis, BR-29075910 Vitoria, ES, Brazil.
[Piattella, Oliver F.] Ist Nazl Fis Nucl, Sez Milano, I-20133 Milan, Italy.
[Pietrobon, Davide] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Giannantonio, Tommaso] Tech Univ Munich, D-85748 Garching, Germany.
[Giannantonio, Tommaso] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
RP Bertacca, D (reprint author), Univ Padua, Dipartimento Fis G Galilei, Via F Marzolo 8, I-35131 Padua, Italy.
EM daniele.bertacca@pd.infn.it; alvise.raccanelli@port.ac.uk;
oliver.piattella@gmail.com; davide.pietrobon@jpl.nasa.gov;
nicola.bartolo@pd.infn.it; sabino.matarrese@pd.infn.it;
tommaso.giannantonio@Universe-cluster.de
RI Piattella, Oliver/J-4373-2013;
OI Piattella, Oliver/0000-0003-4558-0574; Raccanelli,
Alvise/0000-0001-6726-0438; Matarrese, Sabino/0000-0002-2573-1243;
Giannantonio, Tommaso/0000-0002-9865-0436
FU La "Fondazione Ing. Aldo Gini"; ASI [I/016/07/0]; UK Science and
Technology Facilities Research Council (STFC); CNPq [150143/2010-9];
National Aeronautics and Space Administration; Alexander von Humboldt
Foundation
FX DB would like to acknowledge the ICG at the University of Portsmouth for
the hospitality during the development of this project and La
"Fondazione Ing. Aldo Gini" for support. DB research has been partly
supported by ASI contract I/016/07/0 "COFIS". AR is grateful for the
support from a UK Science and Technology Facilities Research Council
(STFC) PhD studentship. OFP research has been supported by the CNPq
contract 150143/2010-9. Part of the research of DP was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration. TG
acknowledges support from the Alexander von Humboldt Foundation. The
authors also thank R. Crittenden, L. Verde, M. Viel for discussions and
suggestions.
NR 82
TC 6
Z9 6
U1 0
U2 3
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 MAR
PY 2011
IS 3
AR 039
DI 10.1088/1475-7516/2011/03/039
PG 24
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 772TE
UT WOS:000291258300039
ER
PT J
AU Datla, RU
Rice, JP
Lykke, KR
Johnson, BC
Butler, JJ
Xiong, X
AF Datla, R. U.
Rice, J. P.
Lykke, K. R.
Johnson, B. C.
Butler, J. J.
Xiong, X.
TI Best Practice Guidelines for Pre-Launch Characterization and Calibration
of Instruments for Passive Optical Remote Sensing
SO JOURNAL OF RESEARCH OF THE NATIONAL INSTITUTE OF STANDARDS AND
TECHNOLOGY
LA English
DT Article
DE best practice guidelines; radiometric calibrations; remote sensing; SI
traceability
ID INFRARED TRANSFER RADIOMETER; EARTH OBSERVING SYSTEM; SPECTRAL
IRRADIANCE; FILTER RADIOMETERS; NIST; MODIS; VALIDATION; FACILITY; MOON;
NM
AB The pre-launch characterization and calibration of remote sensing instruments should be planned and carried out in conjunction with their design and development to meet the mission requirements. The onboard calibrators such as blackbodies and the sensors such as spectral radiometers should be characterized and calibrated using SI traceable standards. In the case of earth remote sensing, this allows inter-comparison and intercalibration of different sensors in space to create global time series of climate records of high accuracy where some inevitable data gaps can be easily bridged. The recommended best practice guidelines for this pre-launch effort is presented based on experience gained at National Institute of Standards and Technology (NIST), National Aeronautics and Space Administration (NASA) and National Oceanic and Atmospheric Administration (NOAA) programs over the past two decades. The currently available radiometric standards and calibration facilities at NIST serving the remote sensing community are described. Examples of best practice calibrations and intercomparisons to build SI (international System of Units) traceable uncertainty budget in the instrumentation used for preflight satellite sensor calibration and validation are presented.
C1 [Datla, R. U.; Johnson, B. C.] Natl Inst Stand & Technol, Opt Technol Div, Gaithersburg, MD 20899 USA.
[Xiong, X.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Butler, J. J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Datla, RU (reprint author), Natl Inst Stand & Technol, Opt Technol Div, Gaithersburg, MD 20899 USA.
EM raju.datla@nist.gov; joe.rice@nist.gov; keith.lykke@nist.gov;
carol.johnson@nist.gov; james.j.butler@nasa.gov;
xiaxiong.xiong-1@nasa.gov
RI Sanders, Susan/G-1957-2011; Butler, James/D-4188-2013
NR 43
TC 7
Z9 8
U1 0
U2 11
PU US GOVERNMENT PRINTING OFFICE
PI WASHINGTON
PA SUPERINTENDENT DOCUMENTS,, WASHINGTON, DC 20402-9325 USA
SN 1044-677X
J9 J RES NATL INST STAN
JI J. Res. Natl. Inst. Stand. Technol.
PD MAR-APR
PY 2011
VL 116
IS 2
BP 621
EP 646
DI 10.6028/jres.116.009
PG 26
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 761ZR
UT WOS:000290442500005
PM 26989588
ER
PT J
AU Sahraoui, F
Goldstein, ML
Abdul-Kader, K
Belmont, G
Rezeau, L
Robert, P
Canu, P
AF Sahraoui, Fouad
Goldstein, Melvyn L.
Abdul-Kader, K.
Belmont, Gerard
Rezeau, Laurence
Robert, Patrick
Canu, Patrick
TI Observation and theoretical modeling of electron scale solar wind
turbulence
SO COMPTES RENDUS PHYSIQUE
LA English
DT Article
DE Solar wind; Turbulence; Dissipation; Cluster; Heating; k-Filtering
ID DISSIPATION RANGE; DYNAMICS; MAGNETOSHEATH; SPECTRA; WAVES
AB Turbulence at MagnetoHydroDynamics (MHD) scales in the solar wind has been studied for more than three decades, using data analysis, theoretical and numerical modeling. However, smaller scales have not been explored until very recently. Here, we review recent results on the first observation of cascade and dissipation of the solar wind turbulence at the electron scales. Thanks to the high resolution magnetic and electric field data of the Cluster spacecraft, we computed the spectra of turbulence up to similar to 100 Hz (in the spacecraft reference frame) and found evidence of energy dissipation around the Doppler-shifted electron gyroscale f(rho e). Before its dissipation, the energy is shown to undergo two cascades: a Kolmogorov-like cascade with a scaling f(-1.6) above the proton gyroscale, and a new f(-2.3) cascade at the sub-proton and electron gyroscales. Above f(rho e) the spectrum has a steeper power law similar to f(-4.1) down to the noise level of the instrument. Solving numerically the linear Maxwell-Vlasov equations combined with recent theoretical predictions of the Gyro-Kinetic theory, we show that the present results are consistent with a scenario of a quasi-two-dimensional cascade into Kinetic Alfven modes (KAW). New analyses of other data sets, where the Cluster separation (of about similar to 200 km) allowed us to explore the sub-proton scales using the k-filtering technique, and to confirm the 2D nature of the turbulence at those scales. (c) 2010 Academie des sciences. Published by Elsevier Masson SAS. All rights reserved.
C1 [Sahraoui, Fouad; Abdul-Kader, K.; Belmont, Gerard; Rezeau, Laurence; Robert, Patrick; Canu, Patrick] Ecole Polytech, Lab Phys Plasmas, CNRS, Observ St Maur, F-94107 St Maur Des Fosses, France.
[Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rezeau, Laurence] Univ Paris 06, F-75005 Paris, France.
RP Sahraoui, F (reprint author), Ecole Polytech, Lab Phys Plasmas, CNRS, Observ St Maur, 4 Ave Nepture, F-94107 St Maur Des Fosses, France.
EM fouad.sahraoui@lpp.polytechnique.fr
RI Goldstein, Melvyn/B-1724-2008
NR 31
TC 8
Z9 8
U1 0
U2 4
PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75724 PARIS, FRANCE
SN 1631-0705
J9 CR PHYS
JI C. R. Phys.
PD MAR
PY 2011
VL 12
IS 2
BP 132
EP 140
DI 10.1016/j.crhy.2010.11.008
PG 9
WC Astronomy & Astrophysics; Physics, Multidisciplinary
SC Astronomy & Astrophysics; Physics
GA 754TQ
UT WOS:000289880700004
ER
PT J
AU Bui, TT
AF Bui, Trong T.
TI Computational Fluid Dynamics Analysis of Nozzle Plume Effects on Sonic
Boom Signature
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 47th AIAA Aerospace Sciences Meeting on New Horizons Forum and Aerospace
Exposition
CY JAN 05-09, 2009
CL Orlando, FL
SP AIAA
ID SCHEME
AB A computational fluid dynamics study is conducted to examine nozzle exhaust jet plume effects on the sonic boom signature of a supersonic aircraft. A simplified axisymmetric nozzle geometry, representative of the nozzle on the NASA Dryden NF-15B Lift and Nozzle Change Effects on Tail Shock research airplane, is considered. The computational fluid dynamics code is validated using available wind-tunnel sonic boom experimental data. The effects of grid size, spatial order of accuracy, grid type, and flow viscosity on the accuracy of the predicted sonic boom pressure signature are quantified. Grid lines parallel to the Mach wave direction are found to give the best results. Second-order-accurate upwind methods are required as a minimum for accurate sonic boom simulations. The highly underexpanded nozzle flow is found to provide significantly more reduction in the tail shock strength in the sonic boom N-wave pressure signature than perfectly expanded and overexpanded nozzle flows. A tail shock train in the sonic boom signature is observed for the highly underexpanded nozzle flow. Axisymmetric computational fluid dynamics simulations show the flow physics inside the F-15 nozzle to be nonisentropic and complex.
C1 NASA, Dryden Flight Res Ctr, Res Aerodynam Prop & Performance Branch, Edwards AFB, CA 93523 USA.
RP Bui, TT (reprint author), NASA, Dryden Flight Res Ctr, Res Aerodynam Prop & Performance Branch, POB 273 MS, Edwards AFB, CA 93523 USA.
NR 16
TC 1
Z9 1
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2011
VL 48
IS 2
BP 368
EP 380
DI 10.2514/1.C000229
PG 13
WC Engineering, Aerospace
SC Engineering
GA 752PT
UT WOS:000289705400002
ER
PT J
AU Bisagni, C
Vescovini, R
Davila, CG
AF Bisagni, Chiara
Vescovini, Riccardo
Davila, Carlos G.
TI Single-Stringer Compression Specimen for the Assessment of Damage
Tolerance of Postbuckled Structures
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 51st AIAA/ASME/ASCE/AHS/ASC Structures Structural Dynamics and Materials
Conference
CY APR 12-15, 2010
CL Orlando, FL
ID STIFFENED PANELS; COMPOSITE; DELAMINATION; SIMULATION; BEHAVIOR; MODEL;
PREDICTION; FRACTURE; COLLAPSE; GROWTH
AB A procedure is proposed for the assessment of the damage tolerance and collapse of stiffened composite panels using a single-stringer compression specimen. The dimensions of the specimen are determined such that the specimen's nonlinear response and collapse are representative of an equivalent multistringer panel in compression. Experimental tests are conducted on specimens with and without an embedded delamination. A shell-based finite element model with intralaminar and interlaminar damage capabilities is developed to predict the postbuckling response as well as the damage evolution from initiation to collapse.
C1 [Bisagni, Chiara; Vescovini, Riccardo] Politecn Milan, Dept Aerosp Engn, I-20156 Milan, Italy.
[Davila, Carlos G.] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Bisagni, C (reprint author), Politecn Milan, Dept Aerosp Engn, Via La Masa 34, I-20156 Milan, Italy.
EM chiara.bisagni@polimi.it; vescovini@aero.polimi.it;
carlos.g.davila@nasa.gov
RI Bisagni, Chiara/G-7158-2012; Vescovini, Riccardo/C-1866-2013; Davila,
Carlos/D-8559-2011
OI Bisagni, Chiara/0000-0002-8713-9763; Vescovini,
Riccardo/0000-0003-3915-5299;
NR 23
TC 7
Z9 7
U1 0
U2 7
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2011
VL 48
IS 2
BP 495
EP 502
DI 10.2514/1.C031106
PG 8
WC Engineering, Aerospace
SC Engineering
GA 752PT
UT WOS:000289705400014
ER
PT J
AU McClain, ST
Tino, P
Kreeger, RE
AF McClain, Stephen T.
Tino, Peter
Kreeger, Richard E.
TI Ice Shape Characterization Using Self-Organizing Maps
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 1st AIAA Atmospheric and Space Environments Conference
CY JUN 22-25, 2009
CL San Antonio, TX
SP Amer Inst Aeronaut & Astronaut
C1 [McClain, Stephen T.] Baylor Univ, Dept Mech Engn, Waco, TX 76798 USA.
[Tino, Peter] Univ Birmingham, Sch Comp Sci, Birmingham B15 2TT, W Midlands, England.
[Kreeger, Richard E.] NASA John H Glenn Res Ctr Lewis Field, Icing Res Branch, Cleveland, OH 44524 USA.
RP McClain, ST (reprint author), Baylor Univ, Dept Mech Engn, 1 Bear Pl 97356, Waco, TX 76798 USA.
NR 7
TC 1
Z9 1
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2011
VL 48
IS 2
BP 724
EP 730
DI 10.2514/1.C031209
PG 7
WC Engineering, Aerospace
SC Engineering
GA 752PT
UT WOS:000289705400040
ER
PT J
AU Miller, SKR
Dever, JA
AF Miller, Sharon K. R.
Dever, Joyce A.
TI Materials International Space Station Experiment 5 Polymer Film Thermal
Control Experiment
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 11th International Symposium on Materials in a Space Environment (ISMSE)
CY SEP, 2009
CL Aix En Provence, FRANCE
SP Ctr Natl Etudes Spatiales (CNES)
AB It is known that polymer films can degrade as a result of space environmental exposure, but the magnitude of the mechanical property degradation and the degree to which the different environmental factors play a role is not well understood. An experiment was flown on the Materials International Space Station Experiment 5 to determine the change in tensile strength and percent elongation of some typical polymer films exposed in a nadir-facing environment on the International Space Station and, where possible, compare with similar ram- and wake-facing experiments flown on the Materials International Space Station Experiment 1 to get a better indication of the role the different environments play in mechanical property change. It was found that the majority of the polymers tested experienced some loss in tensile/yield strength and percent elongation with polytetrafluroethylene Teflon having the greatest change. Where comparisons could be made with the Materials International Space Station Experiment 1, it appears that the loss in percent elongation is dependent on the radiation level while the loss in tensile strength is not as sensitive to the level of radiation.
C1 [Miller, Sharon K. R.] NASA, John H Glenn Res Ctr, Lewis Field, Space Environm & Expt Branch, Cleveland, OH 44135 USA.
[Dever, Joyce A.] NASA, John H Glenn Res Ctr, Lewis Field, Durabil & Protect Coatings Branch, Cleveland, OH 44135 USA.
RP Miller, SKR (reprint author), NASA, John H Glenn Res Ctr, Lewis Field, Space Environm & Expt Branch, 21000 Brookpk Rd,MS 309-2, Cleveland, OH 44135 USA.
NR 7
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 MAR-APR
PY 2011
VL 48
IS 2
BP 240
EP 245
DI 10.2514/1.49482
PG 6
WC Engineering, Aerospace
SC Engineering
GA 752PV
UT WOS:000289705600004
ER
PT J
AU Liechty, DS
Lewis, M
AF Liechty, Derek S.
Lewis, Mark
TI Electronic Energy Level Transition and Ionization Following the
Quantum-Kinetic Chemistry Model
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 11th International Symposium on Materials in a Space Environment (ISMSE)
CY SEP, 2009
CL Aix-en-Provence, FRANCE
SP Ctr Natl Etudes Spatiales (CNES)
ID SIMULATION MONTE-CARLO; NITROGEN
AB A new method of treating electronic energy level transitions as well as linking ionization to electronic energy levels is proposed following the quantum-kinetic chemistry model of Bird. Although the use of electronic energy levels and ionization reactions in direct simulation Monte Carlo method are not new ideas, the current method of selecting what level to transition to, how to reproduce transition rates, and the linking of the electronic energy levels to ionization are, to the author's knowledge, novel concepts. The resulting equilibrium temperatures are shown to remain constant, and the electronic energy level distributions are shown to reproduce the Boltzmann distribution. The electronic energy level transition rates and ionization rates due to electron impacts are shown to reproduce theoretical and measured rates. The rates due to heavy particle impacts, while not as favorable as the electron impact rates, compare favorably to values from the literature. Thus, these new extensions to the quantum-kinetic chemistry model of Bird provide an accurate method for predicting electronic energy level transition and ionization rates in gases. Because these methods are not dependent upon any equilibrium I ate equations or the macroscopic temperature of the gas, they are more appropriate for nonequilibrium flows.
C1 [Liechty, Derek S.; Lewis, Mark] Univ Maryland, College Pk, MD 20742 USA.
[Liechty, Derek S.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Liechty, DS (reprint author), Univ Maryland, College Pk, MD 20742 USA.
NR 22
TC 1
Z9 1
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2011
VL 48
IS 2
BP 283
EP 290
DI 10.2514/1.48826
PG 8
WC Engineering, Aerospace
SC Engineering
GA 752PV
UT WOS:000289705600009
ER
PT J
AU Jiang, HB
Rodriguez, LF
Bell, S
Kortenkamp, D
Capristan, F
AF Jiang, Haibei
Rodriguez, Luis F.
Bell, Scott
Kortenkamp, David
Capristan, Francisco
TI Prediction of Reliability for Environmental Control and Life Support
Systems
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB An increasing awareness of life-support system reliability has been noticed in the aerospace community as long-term space missions become realistic objectives. Literature review indicates a significant knowledge gap in the accurate evaluation of the reliability of environmental control and life-support systems. Quantitative determination of system reliability, however, is subject to large data requirements, often limiting their applicability. In an effort to address this issue, this paper presents an approach to reliability analysis for life-support system design. A simulation tool has been developed with the capability of representing complex dynamic systems with configurable failure rate functions for life-support hardware. This tool has been applied and compared with classical reliability prediction approaches. As a result of this work, it has been determined that typical life-support system configurations are likely to be more reliable than classical approaches might suggest. This is due to an inherent buffering capacity in life-support system design, which might be leveraged to improve the cost effectiveness of future life-support system design.
C1 [Jiang, Haibei; Rodriguez, Luis F.] Univ Illinois, Urbana, IL 61801 USA.
[Bell, Scott; Kortenkamp, David] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Capristan, Francisco] Georgia Inst Technol, Atlanta, GA 30332 USA.
RP Rodriguez, LF (reprint author), Dept Agr & Biol Engn, 376C Agr Engn Sci Bldg,MC-644,1304 W Penn Ave, Urbana, IL 61822 USA.
FU University of Illinois; National Aeronautics and Space Administration;
National Science Foundation; Illinois Space Grant Consortium
FX The authors would gratefully like to acknowledge the generosity of the
University of Illinois, the National Aeronautics and Space
Administration, the National Science Foundation, and the Illinois Space
Grant Consortium in support of this work. The authors would also like to
thank several individuals who also contributed to this work,
particularly Izaak Neveln, David Kane. and Christian Douglass, who
supported this work while partaking in an National Science Foundation
Research Experience for Undergraduates.
NR 20
TC 1
Z9 1
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2011
VL 48
IS 2
BP 336
EP 345
DI 10.2514/1.44792
PG 10
WC Engineering, Aerospace
SC Engineering
GA 752PV
UT WOS:000289705600014
ER
PT J
AU Schurch, MPE
Coe, MJ
McBride, VA
Townsend, LJ
Udalski, A
Haberl, F
Corbet, RHD
AF Schurch, M. P. E.
Coe, M. J.
McBride, V. A.
Townsend, L. J.
Udalski, A.
Haberl, F.
Corbet, R. H. D.
TI Orbital period determinations for four SMC Be/X-ray binaries
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: emission-line, Be; Magellanic Clouds; X-rays: binaries
AB We present an optical and X-ray study of four Be/X-ray binaries located in the Small Magellanic Cloud (SMC). OGLE I-band data of up to 11 years of semicontinuous monitoring has been analysed for SMC X-2, SXP172 and SXP202B, providing both a measurement of the orbital period (P-orb = 18.62, 68.90 and 229.9 d for the pulsars, respectively) and a detailed optical orbital profile for each pulsar. For SXP172 this has allowed a direct comparison of the optical and X-ray emission seen through regular RXTE monitoring, revealing that the X-ray outbursts precede the optical by around 7 d. Recent X-ray studies by XMM-Newton have identified a new source in the vicinity of SXP15.3 raising doubt on the identification of the optical counterpart to this X-ray pulsar. Here we present a discussion of the observations that led to the proposal of the original counterpart and a detailed optical analysis of the counterpart to the new X-ray source, identifying a 21.7 d periodicity in the OGLE I-band data. The optical characteristics of this star are consistent with that of a SMC Be/X-ray binary. However, this star was rejected as the counterpart to SXP15.3 in previous studies due to the lack of H alpha emission.
C1 [Schurch, M. P. E.] Univ Cape Town, Dept Astron, ACGC, ZA-7701 Rondebosch, South Africa.
[Coe, M. J.; McBride, V. A.; Townsend, L. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Haberl, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Corbet, R. H. D.] Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Schurch, MPE (reprint author), Univ Cape Town, Dept Astron, ACGC, Private Bag 11, ZA-7701 Rondebosch, South Africa.
EM schurch@ast.uct.ac.za
OI Haberl, Frank/0000-0002-0107-5237
FU UCT/URC; Polish MNiSW [N20303032/4275]; University of Southampton
FX MPES is supported through the UCT/URC Postdoctoral Research Fellowship.
The OGLE project was partially supported by the Polish MNiSW grant
N20303032/4275. LJT is supported by a Mayflower Scholarship from the
University of Southampton.
NR 0
TC 8
Z9 8
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2011
VL 412
IS 1
BP 391
EP 400
DI 10.1111/j.1365-2966.2010.17914.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 734YC
UT WOS:000288378100033
ER
PT J
AU Mikellides, IG
Katz, I
Hofer, RR
Goebel, DM
de Grys, K
Mathers, A
AF Mikellides, Ioannis G.
Katz, Ira
Hofer, Richard R.
Goebel, Dan M.
de Grys, Kristi
Mathers, Alex
TI Magnetic shielding of the channel walls in a Hall plasma accelerator
SO PHYSICS OF PLASMAS
LA English
DT Article
ID ELECTRON EMISSION; BOHM CRITERION; HOLLOW-CATHODE; MODEL; THRUSTER;
DISCHARGE; SIMULATIONS; PROPULSION; TURBULENCE; SHEATH
AB In a qualification life test of a Hall thruster it was found that the erosion of the acceleration channel practically stopped after similar to 5600 h. Numerical simulations using a two-dimensional axisymmetric plasma solver with a magnetic field-aligned mesh reveal that when the channel receded from its early-in-life to its steady-state configuration the following changes occurred near the wall: (1) reduction of the electric field parallel to the wall that prohibited ions from acquiring significant impact kinetic energy before entering the sheath, (2) reduction of the potential fall in the sheath that further diminished the total energy ions gained before striking the material, and (3) reduction of the ion number density that decreased the flux of ions to the wall. All these changes, found to have been induced by the magnetic field, constituted collectively an effective shielding of the walls from any significant ion bombardment. Thus, we term this process in Hall thrusters "magnetic shielding." (C) 2011 American Institute of Physics. [doi:10.1063/1.3551583]
C1 [Mikellides, Ioannis G.; Katz, Ira; Hofer, Richard R.; Goebel, Dan M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Grys, Kristi; Mathers, Alex] Aerojet, Redmond, WA 98052 USA.
RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ioannis.g.mikellides@jpl.nasa.gov
FU National Aeronautics and Space Administration
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.
Reference herein to any specific commercial product, process, or service
by trade name, trademark, manufacturer, or otherwise does not constitute
or imply its endorsement by the United States Government or the Jet
Propulsion Laboratory, California Institute of Technology.
NR 55
TC 31
Z9 31
U1 1
U2 18
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 MAR
PY 2011
VL 18
IS 3
AR 033501
DI 10.1063/1.3551583
PG 18
WC Physics, Fluids & Plasmas
SC Physics
GA 745FS
UT WOS:000289151900070
ER
PT J
AU Itoh, Y
Oasa, Y
Funayama, H
Hayashi, M
Fukagawa, M
Hashiguchi, T
Currie, T
AF Itoh, Yoichi
Oasa, Yumiko
Funayama, Hitoshi
Hayashi, Masahiko
Fukagawa, Misato
Hashiguchi, Toshio
Currie, Thayne
TI Near-infrared imaging survey of faint companions around young dwarfs in
the Pleiades cluster
SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS
LA English
DT Article
DE planetary systems: formation; techniques: high angular resolution
ID ADAPTIVE OPTICS; INTERSTELLAR EXTINCTION; GIANT PLANETS; STARS; MASS;
IMAGER; CIAO
AB We conducted a near-infrared imaging survey of 11 young dwarfs in the Pleiades cluster using the Subaru Telescope and the near-infrared coronagraph imager. We found ten faint point sources, with magnitudes as faint as 20 mag in the K-band, with around seven dwarfs. Comparison with the Spitzer archive images revealed that a pair of the faint sources around V 1171 Tau is very red in infrared wavelengths, which indicates very low-mass young stellar objects. However, the results of our follow-up proper motion measurements implied that the central star and the faint sources do not share common proper motions, suggesting that they are not physically associated.
C1 [Itoh, Yoichi; Funayama, Hitoshi; Hashiguchi, Toshio] Kobe Univ, Grad Sch Sci, Nada Ku, Kobe, Hyogo 6578501, Japan.
[Oasa, Yumiko] Saitama Univ, Fac Educ, Sakura Ku, Saitama 3388570, Japan.
[Hayashi, Masahiko] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Hayashi, Masahiko] Grad Univ Adv Studies Sokendai, Sch Math & Phys Sci, Mitaka, Tokyo 1818588, Japan.
[Fukagawa, Misato] Osaka Univ, Grad Sch Sci, Osaka 5600043, Japan.
[Currie, Thayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Itoh, Y (reprint author), Kobe Univ, Grad Sch Sci, Nada Ku, 1-1 Rokkodai, Kobe, Hyogo 6578501, Japan.
EM yitoh@kobe-u.ac.jp
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT),
Japan; [16740256]
FX We are grateful to S. Harasawa for the observations. This work is partly
supported by "The 21st Century CUE program: The Origin and Evolution of
Planetary Systems" of the Ministry of Education, Culture, Sports,
Science and Technology (MEXT), Japan. Y.I. is supported by a
Grant-in-Aid for Scientific Research No. 16740256.
NR 26
TC 3
Z9 3
U1 2
U2 3
PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
PI BEIJING
PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA
SN 1674-4527
J9 RES ASTRON ASTROPHYS
JI Res. Astron. Astrophys.
PD MAR
PY 2011
VL 11
IS 3
BP 335
EP 344
DI 10.1088/1674-4527/11/3/007
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 749FH
UT WOS:000289448700007
ER
PT J
AU Lance, KT
Georgiadou, YP
Bregt, AK
AF Lance, K. T.
Georgiadou, Y. P.
Bregt, A. K.
TI Evaluation of the Dutch subsurface geoportal: What lies beneath?
SO COMPUTERS ENVIRONMENT AND URBAN SYSTEMS
LA English
DT Article
DE Geoportal; Governance; Accountability; Autonomy; Result control
ID INFORMATION-SYSTEMS; ORGANIZATION
AB This paper focuses on a geoportal from a "what lies beneath" perspective. It analyses processes of budgeting, planning, monitoring, performance measurement, and reporting of the national initiative titled Digital Information of the Dutch Subsurface (known by its Dutch acronym, DINO). The study is used as a means to empirically refine a conceptual model that illuminates how external agents influence or control the coordination of geo-information in the public sector. DINO is developed and maintained in a formal principal-agent relationship with clear objectives and accountability. DINO is managed by the Netherlands Institute of Applied Geoscience (the agent) through a performance-based management contract with the sponsoring Geo-Information Commission (the principals). The DINO program is characterized by the pooling of financial resources from five ministries, the internal tracking of activity progression, the routine reporting to the user community, and the regular monitoring and evaluation of DINO by the Geo-Information Commission. The case study reveals that 'soft' rather than 'hard' controls are used and that 'mutual shaping' takes place, with the agent influencing how it is 'controlled' by the principal. However, the management contract still relies on a power disparity and reinforces previous research findings that external parties can influence network/coordination conditions. In-depth case studies such as this work can increase understanding of evaluation in the context of politico-administrative processes and improve researchers' ability to critically compare geoportal initiatives. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Lance, K. T.; Georgiadou, Y. P.] Univ Twente, Int Inst Geoinformat Sci & Earth Observat, NL-7500 AA Enschede, Netherlands.
[Bregt, A. K.] Univ Wageningen & Res Ctr, Ctr Geoinformat, NL-6700 AA Wageningen, Netherlands.
RP Lance, KT (reprint author), NASA, USRA, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM lancekt@aya.yale.edu
RI Georgiadou, Yola/L-2942-2013;
OI Bregt, Arnold/0000-0002-5138-5954
NR 37
TC 2
Z9 2
U1 3
U2 9
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0198-9715
J9 COMPUT ENVIRON URBAN
JI Comput. Environ. Urban Syst.
PD MAR
PY 2011
VL 35
IS 2
BP 150
EP 158
DI 10.1016/j.compenvurbsys.2010.09.002
PG 9
WC Computer Science, Interdisciplinary Applications; Engineering,
Environmental; Environmental Studies; Geography; Operations Research &
Management Science
SC Computer Science; Engineering; Environmental Sciences & Ecology;
Geography; Operations Research & Management Science
GA 742EU
UT WOS:000288924900007
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Atwood, WB
Axelsson, M
Baldini, L
Ballet, J
Barbiellini, G
Baring, MG
Bastieri, D
Baughman, BM
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Burnett, TH
Buson, S
Caliandro, GA
Cameron, RA
Camilo, F
Caraveo, PA
Casandjian, JM
Cecchi, C
Celik, O
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cognard, I
Cohen-Tanugi, J
Cominsky, LR
Conrad, J
Corbet, R
Cutini, S
den Hartog, PR
Dermer, CD
de Angelis, A
de Luca, A
de Palma, F
Digel, SW
Dormody, M
Silva, EDE
Drell, PS
Dubois, R
Dumora, D
Espinoza, C
Farnier, C
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Frailis, M
Freire, PCC
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giavitto, G
Giebels, B
Giglietto, N
Giommi, P
Giordano, F
Glanzman, T
Godfrey, G
Gotthelf, EV
Grenier, IA
Grondin, MH
Grove, JE
Guillemot, L
Guiriec, S
Gwon, C
Hanabata, Y
Harding, AK
Hayashida, M
Hays, E
Hughes, RE
Jackson, MS
Johannesson, G
Johnson, AS
Johnson, RP
Johnson, TJ
Johnson, WN
Johnston, S
Kamae, T
Kanbach, G
Kaspi, VM
Katagiri, H
Kataoka, J
Kawai, N
Kerr, M
Knoedlseder, J
Kocian, ML
Kramer, M
Kuss, M
Lande, J
Latronico, L
Lemoine-Goumard, M
Livingstone, M
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Lyne, AG
Madejski, GM
Makeev, A
Manchester, RN
Marelli, M
Mazziotta, MN
McConville, W
McEnery, JE
McGlynn, S
Meurer, C
Michelson, PF
Mineo, T
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Nolan, PL
Norris, JP
Noutsos, A
Nuss, E
Ohsugi, T
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Rando, R
Ransom, SM
Ray, PS
Razzano, M
Rea, N
Reimer, A
Reimer, O
Reposeur, T
Ritz, S
Rodriguez, AY
Romani, RW
Roth, M
Ryde, F
Sadrozinski, HFW
Sanchez, D
Sander, A
Parkinson, PMS
Scargle, JD
Schalk, TL
Sellerholm, A
Sgro, C
Siskind, EJ
Smith, DA
Smith, PD
Spandre, G
Spinelli, P
Stappers, BW
Starck, JL
Striani, E
Strickman, MS
Strong, AW
Suson, DJ
Tajima, H
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JB
Thayer, JG
Theureau, G
Thompson, DJ
Thorsett, SE
Tibaldo, L
Tibolla, O
Torres, DF
Tosti, G
Tramacere, A
Uchiyama, Y
Usher, TL
Van Etten, A
Vasileiou, V
Venter, C
Vilchez, N
Vitale, V
Waite, AP
Wang, P
Wang, N
Watters, K
Weltevrede, P
Winer, BL
Wood, KS
Ylinen, T
Ziegler, M
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Atwood, W. B.
Axelsson, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Baring, M. G.
Bastieri, D.
Baughman, B. M.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Burnett, T. H.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Camilo, F.
Caraveo, P. A.
Casandjian, J. M.
Cecchi, C.
Celik, Oe.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cognard, I.
Cohen-Tanugi, J.
Cominsky, L. R.
Conrad, J.
Corbet, R.
Cutini, S.
den Hartog, P. R.
Dermer, C. D.
de Angelis, A.
de Luca, A.
de Palma, F.
Digel, S. W.
Dormody, M.
do Couto e Silva, E.
Drell, P. S.
Dubois, R.
Dumora, D.
Espinoza, C.
Farnier, C.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Frailis, M.
Freire, P. C. C.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giavitto, G.
Giebels, B.
Giglietto, N.
Giommi, P.
Giordano, F.
Glanzman, T.
Godfrey, G.
Gotthelf, E. V.
Grenier, I. A.
Grondin, M. -H.
Grove, J. E.
Guillemot, L.
Guiriec, S.
Gwon, C.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hays, E.
Hughes, R. E.
Jackson, M. S.
Johannesson, G.
Johnson, A. S.
Johnson, R. P.
Johnson, T. J.
Johnson, W. N.
Johnston, S.
Kamae, T.
Kanbach, G.
Kaspi, V. M.
Katagiri, H.
Kataoka, J.
Kawai, N.
Kerr, M.
Knoedlseder, J.
Kocian, M. L.
Kramer, M.
Kuss, M.
Lande, J.
Latronico, L.
Lemoine-Goumard, M.
Livingstone, M.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Lyne, A. G.
Madejski, G. M.
Makeev, A.
Manchester, R. N.
Marelli, M.
Mazziotta, M. N.
McConville, W.
McEnery, J. E.
McGlynn, S.
Meurer, C.
Michelson, P. F.
Mineo, T.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Nolan, P. L.
Norris, J. P.
Noutsos, A.
Nuss, E.
Ohsugi, T.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Ransom, S. M.
Ray, P. S.
Razzano, M.
Rea, N.
Reimer, A.
Reimer, O.
Reposeur, T.
Ritz, S.
Rodriguez, A. Y.
Romani, R. W.
Roth, M.
Ryde, F.
Sadrozinski, H. F. -W.
Sanchez, D.
Sander, A.
Parkinson, P. M. Saz
Scargle, J. D.
Schalk, T. L.
Sellerholm, A.
Sgro, C.
Siskind, E. J.
Smith, D. A.
Smith, P. D.
Spandre, G.
Spinelli, P.
Stappers, B. W.
Starck, J. -L.
Striani, E.
Strickman, M. S.
Strong, A. W.
Suson, D. J.
Tajima, H.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. B.
Thayer, J. G.
Theureau, G.
Thompson, D. J.
Thorsett, S. E.
Tibaldo, L.
Tibolla, O.
Torres, D. F.
Tosti, G.
Tramacere, A.
Uchiyama, Y.
Usher, T. L.
Van Etten, A.
Vasileiou, V.
Venter, C.
Vilchez, N.
Vitale, V.
Waite, A. P.
Wang, P.
Wang, N.
Watters, K.
Weltevrede, P.
Winer, B. L.
Wood, K. S.
Ylinen, T.
Ziegler, M.
TI THE FIRST FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS (vol
187, pg 460, 2010)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Correction
C1 [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Gwon, C.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Ray, P. S.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Abdo, A. A.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Romani, R. W.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Waite, A. P.; Wang, P.; Watters, K.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Romani, R. W.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Waite, A. P.; Wang, P.; Watters, K.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.; Dormody, M.; Johnson, R. P.; Porter, T. A.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Thorsett, S. E.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Dormody, M.; Johnson, R. P.; Porter, T. A.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Thorsett, S. E.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Conrad, J.; Jackson, M. S.; McGlynn, S.; Meurer, C.; Ryde, F.; Sellerholm, A.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Omodei, N.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Starck, J. -L.; Tibaldo, L.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Giavitto, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Bastieri, D.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Baughman, B. M.; Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; Caliandro, G. A.; 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.; Caliandro, G. A.; 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.; Caliandro, G. A.; 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.; Giebels, B.; Sanchez, D.] CNRS IN2P3, Lab Leprince Ringuet, Ecole Polytech, Palaiseau, France.
[Burnett, T. H.; Kerr, M.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Camilo, F.; Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Caraveo, P. A.; de Luca, A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Celik, Oe.; Moiseev, A. A.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe.; Corbet, R.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Makeev, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Cognard, I.; Theureau, G.] CNRS, Lab Phys & Chem Environm, LPCE UMR 6115, F-45071 Orleans, France.
[Cognard, I.; Theureau, G.] Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Cohen-Tanugi, J.; Farnier, C.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS IN2P3, Montpellier, France.
[Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Conrad, J.; Jackson, M. S.; Meurer, C.; Sellerholm, A.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana Sci Data Ctr, I-00044 Rome, Italy.
[de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[de Luca, A.] IUSS, I-27100 Pavia, Italy.
[Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France.
[Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] CEN Bordeaux Gradignan, CNRS IN2P3, UMR 5797, F-33175 Gradignan, France.
[Espinoza, C.; Kramer, M.; Lyne, A. G.; Noutsos, A.; Stappers, B. W.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Freire, P. C. C.] Arecibo Observ, Arecibo, PR 00612 USA.
[Fukazawa, Y.; Hanabata, Y.; Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Gehrels, N.; Johnson, T. J.; McConville, W.; Moiseev, A. A.] Univ Maryland, Dept Phys & Astron, College Pk, MD 20742 USA.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Jackson, M. S.; McGlynn, S.; Ryde, F.; Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Johnston, S.; Manchester, R. N.; Weltevrede, P.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Kanbach, G.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kaspi, V. M.; Livingstone, M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Kataoka, J.; Kawai, N.; Nakamori, T.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698050, Japan.
[Kawai, N.] Inst Phys & Chem Res RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Mineo, T.] IASF Palermo, I-90146 Palermo, Italy.
[Morselli, A.; Striani, E.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ozaki, M.; Takahashi, T.; Uchiyama, Y.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Rea, N.; Rodriguez, A. Y.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Rea, N.] Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[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.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Striani, E.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tibolla, O.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Torres, D. F.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Tramacere, A.] CIFS, I-10133 Turin, Italy.
[Venter, C.] North West Univ, ZA-2520 Potchefstroom, South Africa.
[Wang, N.] Natl Astron Observ CAS, Urumqi 830011, Peoples R China.
[Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden.
RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM andrea.caliandro@ba.infn.it; elizabeth.c.ferrara@nasa.gov;
parent@cenbg.in2p3.fr; rwr@astro.stanford.edu
RI Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Venter,
Christo/E-6884-2011; Funk, Stefan/B-7629-2015; Rea, Nanda/I-2853-2015;
Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015;
Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta,
Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres,
Diego/O-9422-2016; Orlando, E/R-5594-2016; Starck, Jean-Luc/D-9467-2011;
Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Gehrels,
Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012;
lubrano, pasquale/F-7269-2012; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Reimer,
Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013;
Rando, Riccardo/M-7179-2013
OI Venter, Christo/0000-0002-2666-4812; Funk, Stefan/0000-0002-2012-0080;
Rea, Nanda/0000-0003-2177-6388; Johannesson,
Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673;
Gargano, Fabio/0000-0002-5055-6395; Moskalenko,
Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Starck, Jean-Luc/0000-0003-2177-7794;
Thompson, David/0000-0001-5217-9135; lubrano,
pasquale/0000-0003-0221-4806; giglietto, nicola/0000-0002-9021-2888;
Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385;
NR 2
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2011
VL 193
IS 1
DI 10.1088/0067-0049/193/1/22
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 743ZF
UT WOS:000289059000022
ER
PT J
AU Manoj, P
Kim, KH
Furlan, E
McClure, MK
Luhman, KL
Watson, DM
Espaillat, C
Calvet, N
Najita, JR
D'Alessio, P
Adame, L
Sargent, BA
Forrest, WJ
Bohac, C
Green, JD
Arnold, LA
AF Manoj, P.
Kim, K. H.
Furlan, E.
McClure, M. K.
Luhman, K. L.
Watson, Dan M.
Espaillat, C.
Calvet, N.
Najita, J. R.
D'Alessio, P.
Adame, L.
Sargent, B. A.
Forrest, W. J.
Bohac, C.
Green, J. D.
Arnold, L. A.
TI SPITZER INFRARED SPECTROGRAPH SURVEY OF YOUNG STARS IN THE CHAMAELEON I
STAR-FORMING REGION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; infrared: stars; protoplanetary disks; stars:
pre-main sequence
ID T-TAURI STARS; MAIN-SEQUENCE STARS; LOW-MASS STARS; SPECTRAL
ENERGY-DISTRIBUTIONS; NEARBY MOLECULAR CLOUDS; HERBIG AE/BE SYSTEMS;
BROWN DWARF DISKS; ALL-SKY SURVEY; PROTOPLANETARY DISKS; GRAIN-GROWTH
AB We present 5-36 mu m mid-infrared spectra of 82 young stars in the similar to 2 Myr old Chamaeleon I star-forming region, obtained with the Spitzer Infrared Spectrograph (IRS). We have classified these objects into various evolutionary classes based on their spectral energy distributions and the spectral features seen in the IRS spectra. We have analyzed the mid-IR spectra of Class II objects in Chamaeleon I in detail, in order to study the vertical and radial structure of the protoplanetary disks surrounding these stars. We find evidence for substantial dust settling in most protoplanetary disks in Chamaeleon I. We have identified several disks with altered radial structures in Chamaeleon I, among them transitional disk candidates which have holes or gaps in their disks. Analysis of the silicate emission features in the IRS spectra of Class II objects in Cha I shows that the dust grains in these disks have undergone significant processing (grain growth and crystallization). However, disks with radial holes/gaps appear to have relatively unprocessed grains. We further find the crystalline dust content in the inner (less than or similar to 1-2 AU) and the intermediate (less than or similar to 10 AU) regions of the protoplanetary disks to be tightly correlated. We also investigate the effects of accretion and stellar multiplicity on the disk structure and dust properties. Finally, we compare the observed properties of protoplanetary disks in Cha I with those in slightly younger Taurus and Ophiuchus regions and discuss the effects of disk evolution in the first 1-2 Myr.
C1 [Manoj, P.; Kim, K. H.; Watson, Dan M.; Forrest, W. J.; Bohac, C.; Arnold, L. A.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Furlan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McClure, M. K.; Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Luhman, K. L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Luhman, K. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Espaillat, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Najita, J. R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[D'Alessio, P.; Adame, L.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Sargent, B. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Green, J. D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Manoj, P (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
EM manoj@pas.rochester.edu
OI McClure, Melissa/0000-0003-1878-327X; Adame, Lucia/0000-0002-6328-6099;
Furlan, Elise/0000-0001-9800-6248
FU NASA [1407, 1257184]; JPL/Caltech, JPL [960803]; Cornell [31419-5714];
National Science Foundation [AST-0544588, 0901947]; Pennsylvania State
University; Eberly College of Science; Pennsylvania Space Grant
Consortium; PAPIIT-UNAM, Mexico
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), under NASA contract 1407.
Support for this work was provided by NASA through contract no. 1257184
issued by JPL/Caltech, JPL contract 960803 to Cornell University, and
Cornell subcontracts 31419-5714 to the University of Rochester. E. F.
was partly supported by a NASA Postdoctoral Program Fellowship,
administered by Oak Ridge Associated Universities through a contract
with NASA, and partly supported by NASA through the Spitzer Space
Telescope Fellowship Program, through a contract issued by JPL/Caltech
under a contract with NASA. K. L. was supported by grant AST-0544588
from the National Science Foundation. 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.
C. E. was supported by the National Science Foundation under Award No.
0901947. P. D. acknowledges a grant from PAPIIT-UNAM, Mexico. This
publication makes use of the SIMBAD and VizieR databases, operated at
CDS (Strasbourg, France) and NASA's Astrophysics Data System Abstract
Service.
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SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2011
VL 193
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DI 10.1088/0067-0049/193/1/11
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SC Astronomy & Astrophysics
GA 743ZF
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ER
PT J
AU Mitra, S
Rocha, G
Gorski, KM
Huffenberger, KM
Eriksen, HK
Ashdown, MAJ
Lawrence, CR
AF Mitra, S.
Rocha, G.
Gorski, K. M.
Huffenberger, K. M.
Eriksen, H. K.
Ashdown, M. A. J.
Lawrence, C. R.
TI FAST PIXEL SPACE CONVOLUTION FOR COSMIC MICROWAVE BACKGROUND SURVEYS
WITH ASYMMETRIC BEAMS AND COMPLEX SCAN STRATEGIES: FEBeCoP
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic background radiation; methods: data analysis
ID PRE-LAUNCH STATUS; LOW-FREQUENCY INSTRUMENT; POWER SPECTRUM; NONCIRCULAR
BEAM; PLANCK MISSION; ANISOTROPY; MAPS; DECONVOLUTION; TEMPERATURE;
OPTICS
AB Precise measurement of the angular power spectrum of the cosmic microwave background (CMB) temperature and polarization anisotropy can tightly constrain many cosmological models and parameters. However, accurate measurements can only be realized in practice provided all major systematic effects have been taken into account. Beam asymmetry, coupled with the scan strategy, is a major source of systematic error in scanning CMB experiments such as Planck, the focus of our current interest. We envision Monte Carlo methods to rigorously study and account for the systematic effect of beams in CMB analysis. Toward that goal, we have developed a fast pixel space convolution method that can simulate sky maps observed by a scanning instrument, taking into account real beam shapes and scan strategy. The essence is to pre-compute the "effective beams" using a computer code, "Fast Effective Beam Convolution in Pixel space" (FEBeCoP), that we have developed for the Planck mission. The code computes effective beams given the focal plane beam characteristics of the Planck instrument and the full history of actual satellite pointing, and performs very fast convolution of sky signals using the effective beams. In this paper, we describe the algorithm and the computational scheme that has been implemented. We also outline a few applications of the effective beams in the precision analysis of Planck data, for characterizing the CMB anisotropy and for detecting and measuring properties of point sources.
C1 [Mitra, S.; Rocha, G.; Gorski, K. M.; Lawrence, C. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Ashdown, M. A. J.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
RP Mitra, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sanjit.Mitra@jpl.nasa.gov; graca@caltech.edu;
Krzysztof.M.Gorski@jpl.nasa.gov; huffenbe@physics.miami.edu;
h.k.k.eriksen@astro.uio.no; maja1@mrao.cam.ac.uk;
Charles.R.Lawrence@jpl.nasa.gov
OI Huffenberger, Kevin/0000-0001-7109-0099
FU National Aeronautics and Space Administration
FX We thank B. Crill, M. Seiffert, and F. Bouchet for useful discussions on
Planck beams. We acknowledge C. Cantalupo and T. Kisner for support with
MADcap3 interface, I. O'Dwyer for assistance in devising data formats
for storage of effective beams, and R. Keskitalo for aid in usage of
MADAM mapmaker. Part of the research described in this paper was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
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J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2011
VL 193
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DI 10.1088/0067-0049/193/1/5
PG 17
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SC Astronomy & Astrophysics
GA 743ZF
UT WOS:000289059000005
ER
PT J
AU Moor, A
Pascucci, I
Kospal, A
Abraham, P
Csengeri, T
Kiss, LL
Apai, D
Grady, C
Henning, T
Kiss, C
Bayliss, D
Juhasz, A
Kovacs, J
Szalai, T
AF Moor, A.
Pascucci, I.
Kospal, A.
Abraham, P.
Csengeri, T.
Kiss, L. L.
Apai, D.
Grady, C.
Henning, Th.
Kiss, Cs.
Bayliss, D.
Juhasz, A.
Kovacs, J.
Szalai, T.
TI STRUCTURE AND EVOLUTION OF DEBRIS DISKS AROUND F-TYPE STARS. I.
OBSERVATIONS, DATABASE, AND BASIC EVOLUTIONARY ASPECTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; infrared: stars
ID MULTIBAND IMAGING PHOTOMETER; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE
STARS; SUN-LIKE STARS; TERRESTRIAL PLANET FORMATION; URSA-MAJOR GROUP;
SOLAR-TYPE STARS; HIGH-RESOLUTION SPECTROSCOPY; GENEVA-COPENHAGEN
SURVEY; VEGA-LIKE STARS
AB Although photometric and spectroscopic surveys with the Spitzer Space Telescope remarkably increased the number of well-studied debris disks around A-type and Sun-like stars, detailed analyses of debris disks around F-type stars remained less frequent. Using the MIPS camera and the Infrared Spectrograph (IRS) spectrograph, we searched for debris dust around 82 F-type stars with Spitzer. We found 27 stars that harbor debris disks, nine of which are new discoveries. The dust distribution around two of our stars, HD 50571 and HD 170773, was found to be marginally extended on the 70 mu m MIPS images. Combining the MIPS and IRS measurements with additional infrared and submillimeter data, we achieved excellent spectral coverage for most of our debris systems. We have modeled the excess emission of 22 debris disks using a single temperature dust ring model and of five debris systems with two-temperature models. The latter systems may contain two dust rings around the star. In accordance with the expected trends, the fractional luminosity of the disks declines with time, exhibiting a decay rate consistent with the range of model predictions. We found the distribution of radial dust distances as a function of age to be consistent with the predictions of both the self-stirred and the planetary-stirred disk evolution models. A more comprehensive investigation of the evolution of debris disks around F-type stars, partly based on the presented data set, will be the subject of an upcoming paper.
C1 [Moor, A.; Abraham, P.; Kiss, L. L.; Kiss, Cs.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary.
[Pascucci, I.; Apai, D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kospal, A.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Csengeri, T.] CEA DSM, Lab AIM, IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Kiss, L. L.] Univ Sydney, Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2006, Australia.
[Grady, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Grady, C.] Eureka Sci, Oakland, CA 94602 USA.
[Henning, Th.; Juhasz, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Bayliss, D.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia.
[Kovacs, J.] ELTE Univ, Gothard Astrophys Observ, H-9707 Szombathely, Hungary.
[Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary.
RP Moor, A (reprint author), Hungarian Acad Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary.
EM moor@konkoly.hu
RI Bayliss, Daniel/I-4635-2012
FU NASA [1311495]; Hungarian Research Fund [OTKA K81966]; Spitzer NASA/RSA
[1351891]; Netherlands Organization for Scientific Research; Australian
Research Council; University of Sydney; Hungarian Academy of Sciences;
Hungarian OTKA [K76816, MB0C 81013]; FP6 Marie-Curie Research Training
Network Constellation [MRTN-CT-2006-035890]; NASA; INSU/CNRS (France);
MPG (Germany); IGN (Spain); National Aeronautics and Space
Administration; National Science Foundation
FX We thank an anonymous referee for his/her careful comments which
improved the manuscript. Support for this work was provided by NASA
through contract 1311495 to Eureka Scientific. This work was partly
supported by the Hungarian Research Fund OTKA K81966. I. P. and D. A.
acknowledge support through the Spitzer NASA/RSA contract number
1351891. The research of A.K. is supported by the Netherlands
Organization for Scientific Research. L. L. K. has been supported by the
Australian Research Council, the University of Sydney, the "Lendulet"
Young Researchers Program of the Hungarian Academy of Sciences, and the
Hungarian OTKA grants K76816 and MB0C 81013. T.Cs. acknowledges support
from the FP6 Marie-Curie Research Training Network Constellation: the
origin of stellar masses (MRTN-CT-2006-035890). 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. Partly based on observations
carried out with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS
(France), MPG (Germany), and IGN (Spain). We are grateful to the IRAM
staff for help provided during the observations. This research has made
use of the VizieR catalogue access tool, CDS, Strasbourg, France. The
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.
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SC Astronomy & Astrophysics
GA 743ZF
UT WOS:000289059000004
ER
PT J
AU Hill, MJ
Kunz, RF
Medvitz, RB
Handschuh, RF
Long, LN
Noack, RW
Morris, PJ
AF Hill, Matthew J.
Kunz, Robert F.
Medvitz, Richard B.
Handschuh, Robert F.
Long, Lyle N.
Noack, Ralph W.
Morris, Philip J.
TI CFD Analysis of Gear Windage Losses: Validation and Parametric
Aerodynamic Studies
SO JOURNAL OF FLUIDS ENGINEERING-TRANSACTIONS OF THE ASME
LA English
DT Article
ID HIGH-SPEED GEARS; POWER LOSS; SPUR GEAR
AB A computational fluid dynamics (CFD) method has been applied to gear configurations with and without shrouding. The goals of this work have been to validate the numerical and modeling approaches used for these applications and to develop physical understanding of the aerodynamics of gear windage loss. Several spur gear geometries are considered, for which experimental data are available. Various canonical shrouding configurations and free spinning (no shroud) cases are studied. Comparisons are made with experimental data from open literature, and data recently obtained in the NASA Glenn Research Center Gear Windage Test Facility, Cleveland, OH. The results show good agreement with the experiment. The parametric shroud configuration studies carried out in the Glenn experiments and the CFD analyses elucidate the physical mechanisms of windage losses as well as mitigation strategies due to shrouding and newly proposed tooth contour modifications. [DOI: 10.1115/1.4003681]
C1 [Hill, Matthew J.; Long, Lyle N.; Morris, Philip J.] Penn State Univ, Dept Aerosp Engn, University Pk, PA 16802 USA.
[Kunz, Robert F.; Medvitz, Richard B.; Noack, Ralph W.] Penn State Univ, Appl Res Lab, University Pk, PA 16802 USA.
[Handschuh, Robert F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Hill, MJ (reprint author), Penn State Univ, Dept Aerosp Engn, University Pk, PA 16802 USA.
EM mjh414@psu.edu; rfk102@arl.psu.edu; rbm120@arl.psu.edu;
robert.f.handschuh@nasa.gov; lnl@psu.edu; rwn10@arl.psu.edu;
pjmaer@engr.psu.edu
FU NASA [NNX07AB34A]
FX This work was supported by NASA under NASA Cooperative Agreement No.
NNX07AB34A.
NR 23
TC 6
Z9 7
U1 0
U2 9
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0098-2202
EI 1528-901X
J9 J FLUID ENG-T ASME
JI J. Fluids Eng.-Trans. ASME
PD MAR
PY 2011
VL 133
IS 3
AR 031103
DI 10.1115/1.4003681
PG 10
WC Engineering, Mechanical
SC Engineering
GA 741YO
UT WOS:000288904000005
ER
PT J
AU Buenemann, M
Martius, C
Jones, JW
Herrmann, SM
Klein, D
Mulligan, M
Reed, MS
Winslow, M
Washington-Allen, RA
Lal, R
Ojima, D
AF Buenemann, M.
Martius, C.
Jones, J. W.
Herrmann, S. M.
Klein, D.
Mulligan, M.
Reed, M. S.
Winslow, M.
Washington-Allen, R. A.
Lal, R.
Ojima, D.
TI INTEGRATIVE GEOSPATIAL APPROACHES FOR THE COMPREHENSIVE MONITORING AND
ASSESSMENT OF LAND MANAGEMENT SUSTAINABILITY: RATIONALE, POTENTIALS, AND
CHARACTERISTICS
SO LAND DEGRADATION & DEVELOPMENT
LA English
DT Article
DE remote sensing; geographic information systems; geospatial; drylands;
sustainability; land management; land degradation
ID SUB-SAHARAN AFRICA; SPATIAL-ANALYSIS; SOIL-SALINITY; COUPLED HUMAN;
RIVER-BASIN; GIS; MODEL; SYSTEMS; HEALTH; LANDSCAPE
AB Sustainable dryland management seeks to improve the conditions of people and ecosystems affected by degradation, but it is often unclear which land management strategies work, which ones do not and why. Monitoring and assessment (M&A) can support decision-making by providing this information. As implied by the 10-year Strategy of the United Nations Convention to Combat Desertification (UNCCD), however, M&A efforts have thus far been insufficient or inadequate. We argue that integrative geospatial approaches should be implemented to enhance dryland management decision-making. By assimilating and linking human and environmental data, qualitative and quantitative data, as well as field and remotely sensed data in a spatially explicit framework, such approaches facilitate assessments of both the complexities and place-specificities inherent to sustainability. In addition, they help represent different stakeholder perspectives, promote communication among scientists from diverse backgrounds as well as between scientific and local experts, facilitate inter-institutional knowledge sharing, and create synergy between the UNCCD and other Conventions. Due to these benefits as well as the rapid evolution and increasing availability and affordability of geospatial data and technologies in all countries, it is appropriate to begin capitalizing more fully on them now for the M&A of land management sustainability. In order for integrative geospatial approaches to become more central to M&A efforts, however, capacities and infrastructure must be improved and standards and protocols developed for the collection, analysis, and modeling of data, for the evaluation of outputs, and for the reporting of results. Copyright (C) 2010 John Wiley & Sons, Ltd.
C1 [Buenemann, M.] New Mexico State Univ, Dept Geog, Las Cruces, NM 88003 USA.
[Martius, C.] Int Ctr Agr Res Dry Areas, Program Sustainable Agr Dev Cent Asia & Caucasus, Tashkent, Uzbekistan.
[Jones, J. W.] Univ Florida, Dept Agr & Biol Engn, Gainesville, FL 32611 USA.
[Herrmann, S. M.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Biospher Sci Branch, Greenbelt, MD 20171 USA.
[Klein, D.] Univ Wurzburg, Inst Geog, Dept Remote Sensing, D-97074 Wurzburg, Germany.
[Mulligan, M.] Kings Coll London, Dept Geog, Strand, London WC2R 2LS, England.
[Reed, M. S.] Univ Aberdeen, Sch Geosci, Aberdeen Ctr Environm Sustainabil, Aberdeen AB24 3UF, Scotland.
[Reed, M. S.] Univ Aberdeen, Sch Geosci, Ctr Planning & Environm Management, Aberdeen AB24 3UF, Scotland.
[Winslow, M.] Int Crops Res Inst Semi Arid Trop, Patancheru 502324, Andhra Pradesh, India.
[Washington-Allen, R. A.] Texas A&M Univ, Dept Ecosyst Sci & Management, College Stn, TX 77843 USA.
[Lal, R.] Ohio State Univ, Sch Environm & Nat Resources, Carbon Management & Sequestrat Ctr, Columbus, OH 43210 USA.
[Ojima, D.] Colorado State Univ, Nat Resource Ecol Lab, Ft Collins, CO 80523 USA.
RP Buenemann, M (reprint author), New Mexico State Univ, Dept Geog, POB 30001, Las Cruces, NM 88003 USA.
EM elabuen@nmsu.edu
RI Lal, Rattan/D-2505-2013; Ojima, Dennis/C-5272-2016;
OI Reed, Mark/0000-0002-8958-8474; Martius, Christopher/0000-0002-6884-0298
NR 138
TC 13
Z9 13
U1 0
U2 31
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1085-3278
J9 LAND DEGRAD DEV
JI Land Degrad. Dev.
PD MAR-APR
PY 2011
VL 22
IS 2
SI SI
BP 226
EP 239
DI 10.1002/ldr.1074
PG 14
WC Environmental Sciences; Soil Science
SC Environmental Sciences & Ecology; Agriculture
GA 743FR
UT WOS:000289003600007
ER
PT J
AU Dell'Agnello, S
Delle Monache, GO
Currie, DG
Vittori, R
Cantone, C
Garattini, M
Boni, A
Martini, M
Lops, C
Intaglietta, N
Tauraso, R
Arnold, DA
Pearlman, MR
Bianco, G
Zerbini, S
Maiello, M
Berardi, S
Porcelli, L
Alley, CO
McGarry, JF
Sciarretta, C
Luceri, V
Zagwodzki, TW
AF Dell'Agnello, S.
Delle Monache, G. O.
Currie, D. G.
Vittori, R.
Cantone, C.
Garattini, M.
Boni, A.
Martini, M.
Lops, C.
Intaglietta, N.
Tauraso, R.
Arnold, D. A.
Pearlman, M. R.
Bianco, G.
Zerbini, S.
Maiello, M.
Berardi, S.
Porcelli, L.
Alley, C. O.
McGarry, J. F.
Sciarretta, C.
Luceri, V.
Zagwodzki, T. W.
TI Creation of the new industry-standard space test of laser
retroreflectors for the GNSS and LAGEOS
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Galileo; GPS; SLR; New space test; Laser retroreflectors;
Industry-standard; LAGEOS
ID INTERNATIONAL GLONASS EXPERIMENT; SERVICE; PROSPECTS; GEODESY
AB We built a new experimental apparatus (the "Satellite/lunar laser ranging Characterization Facility", SCF) and created a new test procedure (the SCF-Test) to characterize and model the detailed thermal behavior and the optical performance of cube corner laser retroreflectors in space for industrial and scientific applications. The primary goal of these innovative tools is to provide critical design and diagnostic capabilities for Satellites Laser Ranging (SLR) to Galileo and other GNSS (Global Navigation Satellite System) constellations. The capability will allow us to optimize the design of GNSS laser retroreflector payloads to maximize ranging efficiency, to improve signal-to-noise conditions in daylight and to provide pre-launch validation of retroreflector performance under laboratory-simulated space conditions. Implementation of new retroreflector designs being studied will help to improve GNSS orbits, which will then increase the accuracy, stability, and distribution of the International Terrestrial Reference Frame (ITRF), to provide better definition of the geocenter (origin) and the scale (length unit).
Our key experimental innovation is the concurrent measurement and modeling of the optical Far Field Diffraction Pattern (FFDP) and the temperature distribution of the SLR retroreflector payload under thermal conditions produced with a close-match solar simulator. The apparatus includes infrared cameras for non-invasive thermometry, thermal control and real-time movement of the payload to experimentally simulate satellite orientation on orbit with respect to both solar illumination and laser interrogation beams. These unique capabilities provide experimental validation of the space segment for SLR and Lunar Laser Ranging (LLR).
We used the SCF facility and the SCF-Test to perform a comprehensive, non-invasive space characterization of older generation, back-coated retroreflectors of the GIOVE-A and -B (Galileo In-Orbit Validation Elements) and the GPS-35 and -36 designs. First, using a full GPS flight model at laser wavelengths of 532 and 632 nm, we found its "effective optical cross section" in air, under isothermal conditions, to be six times lower than the Retrorefiector Standard for GNSS satellites (100 x 10(6) m(2) at 20,000 km altitude for GPS and 180 x 10(6) m(2) for Galileo at 23,200 km altitude), issued by the International Laser Ranging Service (ILRS). Under the simulated thermal and space conditions of the SCF, we also showed that in some space configurations the "effective optical cross section" is further reduced, by the thermal degradation of the FFDP. Using the same SCF-Test configuration on an individual GIOVE prototype cube, we measured severe thermal degradation in optical performance, which appears to be caused by the retroreflector metal coating and the non-optimized thermal conductance of the mounting.
Uncoated retroreflectors with proper mounting can minimize thermal degradation and significantly increase the optical performance, and as such, are emerging as the recommended design for modern GNSS satellites. The COMPASS-MI, GLONASS-115 GNSS satellites use uncoated cubes. They provide better efficiency than those on GPS and GIOVE, including better daylight ranging performance. However, these retroreflectors were not characterized in the laboratory under space conditions prior to launch, so we have no basis to evaluate how well they were optimized for future GNSS satellites. SCF-Testing, under a non-disclosure agreement between INFN-LNF and the European Space Agency (ESA), of prototype uncoated cubes for the first four Galileo satellites to be launched (named "IOV", In-Orbit Validation satellites) is a major step forward. An SCF-Test performed on a LAGEOS (LAser GEOdynamics Satellite) engineering model retroreflector array provided by NASA, showed the good space performance on what is now a reference ILRS payload standard. The IOV and LAGEOS measurements demonstrated the effectiveness of the SCF-Test as an LRA diagnostic, optimization and validation tool in use by NASA, ESA and ASI. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Dell'Agnello, S.; Delle Monache, G. O.; Cantone, C.; Garattini, M.; Boni, A.; Martini, M.; Lops, C.; Intaglietta, N.; Tauraso, R.; Maiello, M.; Berardi, S.; Porcelli, L.] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Rome, Italy.
[Currie, D. G.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Vittori, R.] Aeronaut Mil Italiana, I-00185 Rome, Italy.
[Vittori, R.] ASI, I-00198 Rome, Italy.
[Tauraso, R.] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy.
[Arnold, D. A.; Pearlman, M. R.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA.
[Bianco, G.; Sciarretta, C.; Luceri, V.] Ctr Geodesia Spaziale G Colombo ASI CGS, ASI, I-75100 Matera, Italy.
[Zerbini, S.] Univ Bologna, Dept Phys, Sector Geophys, I-40127 Bologna, Italy.
[McGarry, J. F.; Zagwodzki, T. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dell'Agnello, S (reprint author), Ist Nazl Fis Nucl, Lab Nazl Frascati, Via E Fermi 40, I-00044 Rome, Italy.
EM Simone.DellAgnello@lnf.infn.it
OI Bianco, Giuseppe/0000-0002-4538-6467; Tauraso,
Roberto/0000-0002-5619-3513; Martini, Manuele/0000-0001-6508-2930
NR 23
TC 17
Z9 17
U1 0
U2 12
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD MAR 1
PY 2011
VL 47
IS 5
BP 822
EP 842
DI 10.1016/j.asr.2010.10.022
PG 21
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 737SS
UT WOS:000288589100006
ER
PT J
AU Elsila, JE
Callahan, MP
Glavin, DP
Dworkin, JP
Bruckner, H
AF Elsila, Jamie E.
Callahan, Michael P.
Glavin, Daniel P.
Dworkin, Jason P.
Brueckner, Hans
TI Distribution and Stable Isotopic Composition of Amino Acids from Fungal
Peptaibiotics: Assessing the Potential for Meteoritic Contamination
SO ASTROBIOLOGY
LA English
DT Article
DE Filamentous fungi; Amino acids; alpha-aminoisobutyric acid;
Contamination; Isotopes
ID ALPHA-AMINOISOBUTYRIC-ACID; MURCHISON METEORITE; CARBONACEOUS
METEORITES; LIQUID-CHROMATOGRAPHY; DEUTERIUM ENRICHMENT;
MASS-SPECTROMETRY; PLANT-RESPONSES; PARENT BODY; EXTRATERRESTRIAL;
TRICHODERMA
AB The presence of nonprotein alpha-dialkyl-amino acids such as alpha-aminoisobutyric acid (alpha-AIB) and isovaline (Iva), which are considered to be relatively rare in the terrestrial biosphere, has long been used as an indication of the indigeneity of meteoritic amino acids. However, recent work showing the presence of alpha-AIB and Iva in peptides produced by a widespread group of filamentous fungi indicates the possibility of a terrestrial biotic source for the alpha-AIB observed in some meteorites. We measured the amino acid distribution and stable carbon and nitrogen isotopic composition of four alpha-AIB-containing fungal peptides and compared this data to similar meteoritic measurements. We show that the relatively simple distribution of the C(4) and C(5) amino acids in fungal peptides is distinct from the complex distribution observed in many carbonaceous chondrites. We also identify potentially diagnostic relationships between the stable isotopic compositions of pairs of amino acids from the fungal peptides that may aid in ruling out fungal contamination as a source of meteoritic amino acids.
C1 [Elsila, Jamie E.; Callahan, Michael P.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Elsila, Jamie E.; Callahan, Michael P.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Brueckner, Hans] Univ Giessen, Interdisciplinary Res Ctr Biosyst Land Use & Nutr, Dept Food Sci, Inst Nutr Sci, Giessen, Germany.
[Brueckner, Hans] King Saud Univ, Dept Food Sci & Nutr, Riyadh, Saudi Arabia.
RP Elsila, JE (reprint author), NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Code 691, Greenbelt, MD 20771 USA.
EM Jamie.Elsila@nasa.gov
RI Elsila, Jamie/C-9952-2012; Callahan, Michael/D-3630-2012; Glavin,
Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012
OI 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 are grateful for funding support from the NASA Astrobiology Institute
and the Goddard Center for Astrobiology, and the NASA Cosmochemistry
Program. M.P.C. acknowledges support from the NASA Postdoctoral Program
at the Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA.
NR 58
TC 20
Z9 20
U1 2
U2 14
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 MAR
PY 2011
VL 11
IS 2
BP 123
EP 133
DI 10.1089/ast.2010.0505
PG 11
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 739DJ
UT WOS:000288693400004
PM 21417942
ER
PT J
AU Johnson, PV
Hodyss, R
Bolser, DK
Bhartia, R
Lane, AL
Kanik, I
AF Johnson, Paul V.
Hodyss, Robert
Bolser, Diana K.
Bhartia, Rohit
Lane, Arthur L.
Kanik, Isik
TI Ultraviolet-Stimulated Fluorescence and Phosphorescence of Aromatic
Hydrocarbons in Water Ice
SO ASTROBIOLOGY
LA English
DT Article
DE Fluorescence; Phosphorescence; Organic detection; Icy worlds
ID SINGLET EMISSION SPECTRA; TITANS ATMOSPHERE; AMINO-ACIDS; DEGREES K;
BENZENE; 77-DEGREES-K; SPECTROSCOPY; METEORITES; MISSION; EUROPA
AB A principal goal of astrobiology is to detect and inventory the population of organic compounds on extraterrestrial bodies. Targets of specific interest include the wealth of icy worlds that populate our Solar System. One potential technique for in situ detection of organics trapped in water ice matrices involves ultraviolet-stimulated emission from these compounds. Here, we report a preliminary investigation into the feasibility of this concept. Specifically, fluorescence and phosphorescence of pure benzene ice and 1% mixtures of benzene, toluene, p-xylene, m-xylene, and o-xylene in water ice, respectively, were studied at temperatures ranging from similar to 17K up to 160 K. Spectra were measured from 200-500 nm (50,000-20,000 cm(-1)) while ice mixtures were excited at 248.6 nm. The temperature dependence of the fluorescence and phosphorescence intensities was found to be independent of the thermal history and phase of the ice matrix in all cases examined. All phosphorescent emissions were found to decrease in intensity with increasing temperature. Similar behavior was observed for fluorescence in pure benzene, while the observed fluorescence intensity in water ices was independent of temperature.
C1 [Johnson, Paul V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
CALTECH, NASA Astrobiol Inst, Pasadena, CA 91109 USA.
RP Johnson, PV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-601, Pasadena, CA 91109 USA.
EM Paul.V.Johnson@jpl.nasa.gov
RI Johnson, Paul/D-4001-2009
OI Johnson, Paul/0000-0002-0186-8456
FU National Aeronautics and Space Administration; internal Research and
Technology Development program; NASA Astrobiology Institute (Icy Worlds)
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration and funded through the internal
Research and Technology Development program. Further, we acknowledge
support from the NASA Astrobiology Institute (Icy Worlds). Our gratitude
is also extended to William Hug/Ray Reid (Photon Systems, Inc.) for the
use of the NeCu hollow cathode laser.
NR 31
TC 3
Z9 3
U1 2
U2 17
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 MAR
PY 2011
VL 11
IS 2
BP 151
EP 156
DI 10.1089/ast.2010.0568
PG 6
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 739DJ
UT WOS:000288693400006
PM 21417944
ER
PT J
AU Summons, RE
Amend, JP
Bish, D
Buick, R
Cody, GD
Des Marais, DJ
Dromart, G
Eigenbrode, JL
Knoll, AH
Sumner, DY
AF Summons, Roger E.
Amend, Jan P.
Bish, David
Buick, Roger
Cody, George D.
Des Marais, David J.
Dromart, Gilles
Eigenbrode, Jennifer L.
Knoll, Andrew H.
Sumner, Dawn Y.
TI Preservation of Martian Organic and Environmental Records: Final Report
of the Mars Biosignature Working Group
SO ASTROBIOLOGY
LA English
DT Article
DE Astrobiology; Atmospheric gases; Mars; Biosignatures; Life detection
ID CITY HYDROTHERMAL FIELD; MERIDIANI-PLANUM; CLAY-MINERALS; AMINO-ACIDS;
CARBONACEOUS METEORITES; ISOTOPIC FRACTIONATION; MURCHISON METEORITE;
OPPORTUNITY ROVER; ABIOTIC SYNTHESIS; SULFATE MINERALS
AB The Mars Science Laboratory (MSL) has an instrument package capable of making measurements of past and present environmental conditions. The data generated may tell us if Mars is, or ever was, able to support life. However, the knowledge of Mars' past history and the geological processes most likely to preserve a record of that history remain sparse and, in some instances, ambiguous. Physical, chemical, and geological processes relevant to biosignature preservation on Earth, especially under conditions early in its history when microbial life predominated, are also imperfectly known. Here, we present the report of a working group chartered by the Co-Chairs of NASA's MSL Project Science Group, John P. Grotzinger and Michael A. Meyer, to review and evaluate potential for biosignature formation and preservation on Mars.
Orbital images confirm that layered rocks achieved kilometer-scale thicknesses in some regions of ancient Mars. Clearly, interplays of sedimentation and erosional processes govern present-day exposures, and our understanding of these processes is incomplete. MSL can document and evaluate patterns of stratigraphic development as well as the sources of layered materials and their subsequent diagenesis. It can also document other potential biosignature repositories such as hydrothermal environments. These capabilities offer an unprecedented opportunity to decipher key aspects of the environmental evolution of Mars' early surface and aspects of the diagenetic processes that have operated since that time.
Considering the MSL instrument payload package, we identified the following classes of biosignatures as within the MSL detection window: organism morphologies (cells, body fossils, casts), biofabrics (including microbial mats), diagnostic organic molecules, isotopic signatures, evidence of biomineralization and bioalteration, spatial patterns in chemistry, and biogenic gases. Of these, biogenic organic molecules and biogenic atmospheric gases are considered the most definitive and most readily detectable by MSL.
C1 [Summons, Roger E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Amend, Jan P.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Bish, David] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Buick, Roger] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Cody, George D.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Des Marais, David J.] NASA Ames Res Ctr, Exobiol Branch, Moffett Field, CA USA.
[Dromart, Gilles] Univ Lyon, CNRS UMR 5276, ENS Lyon, F-69364 Lyon 07, France.
[Eigenbrode, Jennifer L.] NASA Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA.
[Knoll, Andrew H.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Knoll, Andrew H.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Sumner, Dawn Y.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
RP Summons, RE (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM rsummons@mit.edu
RI Sumner, Dawn/E-8744-2011; Eigenbrode, Jennifer/D-4651-2012;
OI Sumner, Dawn/0000-0002-7343-2061; Buick, Roger/0000-0003-0139-1659
NR 98
TC 65
Z9 65
U1 7
U2 64
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 MAR
PY 2011
VL 11
IS 2
BP 157
EP 181
DI 10.1089/ast.2010.0506
PG 25
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 739DJ
UT WOS:000288693400007
PM 21417945
ER
PT J
AU Tariq, MA
Soedipe, A
Ramesh, G
Wu, HL
Zhang, Y
Shishodia, S
Pourmand, N
Jejelowo, O
AF Tariq, Muhammad Akram
Soedipe, Ayodotun
Ramesh, Govindarajan
Wu, Honglu
Zhang, Ye
Shishodia, Shishir
Pourmand, Nader
Jejelowo, Olufisayo
TI The effect of acute dose charge particle radiation on expression of DNA
repair genes in mice
SO MOLECULAR AND CELLULAR BIOCHEMISTRY
LA English
DT Article
DE Charge particle; Radiation; DNA repair genes; Mice
ID STRAND BREAK REPAIR; IONIZING-RADIATION; POLY(ADP-RIBOSE) POLYMERASE-1;
ULTRAVIOLET-RADIATION; NUCLEOTIDE EXCISION; PROTON EVENTS; ATM KINASE;
CELL-CYCLE; DAMAGE; EXPOSURE
AB The space radiation environment consists of trapped particle radiation, solar particle radiation, and galactic cosmic radiation (GCR), in which protons are the most abundant particle type. During missions to the moon or to Mars, the constant exposure to GCR and occasional exposure to particles emitted from solar particle events (SPE) are major health concerns for astronauts. Therefore, in order to determine health risks during space missions, an understanding of cellular responses to proton exposure is of primary importance. The expression of DNA repair genes in response to ionizing radiation (X-rays and gamma rays) has been studied, but data on DNA repair in response to protons is lacking. Using qPCR analysis, we investigated changes in gene expression induced by positively charged particles (protons) in four categories (0, 0.1, 1.0, and 2.0 Gy) in nine different DNA repair genes isolated from the testes of irradiated mice. DNA repair genes were selected on the basis of their known functions. These genes include ERCC1 (5' incision subunit, DNA strand break repair), ERCC2/NER (opening DNA around the damage, Nucleotide Excision Repair), XRCC1 (5' incision subunit, DNA strand break repair), XRCC3 (DNA break and cross-link repair), XPA (binds damaged DNA in preincision complex), XPC (damage recognition), ATA or ATM (activates checkpoint signaling upon double strand breaks), MLH1 (post-replicative DNA mismatch repair), and PARP1 (base excision repair). Our results demonstrate that ERCC1, PARP1, and XPA genes showed no change at 0.1 Gy radiation, up-regulation at 1.0 Gy radiation (1.09 fold, 7.32 fold, 0.75 fold, respectively), and a remarkable increase in gene expression at 2.0 Gy radiation (4.83 fold, 57.58 fold and 87.58 fold, respectively). Expression of other genes, including ATM and XRCC3, was unchanged at 0.1 and 1.0 Gy radiation but showed up-regulation at 2.0 Gy radiation (2.64 fold and 2.86 fold, respectively). We were unable to detect gene expression for the remaining four genes (XPC, ERCC2, XRCC1, and MLH1) in either the experimental or control animals.
C1 [Tariq, Muhammad Akram; Pourmand, Nader] Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA.
[Tariq, Muhammad Akram; Soedipe, Ayodotun; Shishodia, Shishir; Jejelowo, Olufisayo] Texas So Univ, Ctr Bionanotechnol & Environm Res, Houston, TX 77004 USA.
[Soedipe, Ayodotun; Shishodia, Shishir; Jejelowo, Olufisayo] Texas So Univ, Dept Biol, Houston, TX 77004 USA.
[Ramesh, Govindarajan] Norfolk State Univ, Dept Biol, Norfolk, VA 23504 USA.
[Wu, Honglu; Zhang, Ye] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Pourmand, N (reprint author), Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA.
EM pourmand@soe.ucsc.edu
RI Gridley, Daila/P-7711-2015
FU National Aeronautics and Space Administration [NCC9-165, NNX08BA47A];
National Institutes of Health [P01-HG000205]; National Science
Foundation [DBI 0830141]
FX This work was supported in part by grants from the National Aeronautics
and Space Administration Cooperative Agreements NCC9-165 and NNX08BA47A,
National Institutes of Health [P01-HG000205], the National Science
Foundation [DBI 0830141].
NR 45
TC 4
Z9 4
U1 0
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0300-8177
J9 MOL CELL BIOCHEM
JI Mol. Cell. Biochem.
PD MAR
PY 2011
VL 349
IS 1-2
BP 213
EP 218
DI 10.1007/s11010-010-0641-0
PG 6
WC Cell Biology
SC Cell Biology
GA 735FH
UT WOS:000288398300022
PM 21080036
ER
PT J
AU Cady, E
McElwain, M
Kasdin, NJ
Thalmann, C
AF Cady, Eric
McElwain, Michael
Kasdin, N. Jeremy
Thalmann, Christian
TI A Dual-Mask Coronagraph for Observing Faint Companions to Binary Stars
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID BAND-LIMITED MASK; LYOT CORONAGRAPHS; PLANET FORMATION; VORTEX
CORONAGRAPH; CIRCUMBINARY DISCS; IMAGE MASKS; SYSTEMS; MIGRATION; DISKS;
INSTABILITY
AB Observations of binary stars for faint companions with conventional coronagraphic methods are challenging, as both targets will be bright enough to obscure any nearby faint companions if their scattered light is not suppressed. We propose coronagraphic examination of binary stars using an apodized-pupil Lyot coronagraph and a pair of actively controlled image-plane masks to suppress both stars simultaneously. The performance is compared with imaging with a band-limited mask, a dual-mask Lyot coronagraph, and no coronagraph at all. An imaging procedure and control system for the masks are also described.
C1 [Cady, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McElwain, Michael; Kasdin, N. Jeremy] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
[McElwain, Michael] Princeton Univ Observ, Princeton, NJ 08544 USA.
[McElwain, Michael] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Thalmann, Christian] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Cady, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM eric.j.cady@jpl.nasa.gov
RI McElwain, Michael/D-3607-2012
OI McElwain, Michael/0000-0003-0241-8956
FU National Science Foundation [AST-0901967]
FX The authors would like to thank Sebastian Egner for graciously providing
simulated wavefront data, Laurent Pueyo for useful discussions, and Remi
Soummer for providing code for creating apodizers for apodized-pupil
Lyot coronagraphs. M. W. M. acknowledges support from National Science
Foundation Astronomy & Astrophysics Postdoctoral Fellowship under award
AST-0901967.
NR 53
TC 2
Z9 2
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 MAR
PY 2011
VL 123
IS 901
BP 333
EP 340
DI 10.1086/659038
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 738IN
UT WOS:000288633600006
ER
PT J
AU Wu, CC
Lepping, RP
AF Wu, Chin-Chun
Lepping, R. P.
TI Statistical Comparison of Magnetic Clouds with Interplanetary Coronal
Mass Ejections for Solar Cycle 23
SO SOLAR PHYSICS
LA English
DT Article
DE Geomagnetic storm; Interplanetary coronal mass ejection; Magnetic cloud;
Solar cycle
ID INTER-PLANETARY SHOCK; GEOMAGNETIC STORMS; FIELD STRUCTURE; DRIVER GAS;
1 AU; WIND; CMES; PARAMETER
AB We compare the number and characteristics of interplanetary coronal mass ejections (ICMEs) to those of magnetic clouds (MCs) by using in-situ solar wind plasma and magnetic field observations made at 1 AU during solar cycle 23. We found that approximate to 28% of ICMEs appear to contain MCs, since 103 magnetic clouds (MCs) occurred during 1995 - 2006, and 307 ICMEs occurred during 1996-2006. For the period between 1996 and 2006, 85 MCs are identified as part of ICMEs, and six MCs are not associated with ICMEs, which conflicts with the idea that MCs are usually a subset of ICMEs. It was also found that solar wind conditions inside MCs and ICMEs are usually similar, but the linear correlation between geomagnetic storm intensity (Dst(min)) and relevant solar wind parameters is better for MCs than for ICMEs. The differences between average event duration (At) and average proton plasma beta () are two of the major differences between MCs and ICMEs: i) the average duration of ICMEs (29.6 h) is 44% longer than for MCs (20.6 hours), and ii) the average of is 0.01 for MCs and 0.24 for ICMEs. The difference between the definition of a MC and that for an ICME is one of the major reasons for these average characteristics being different (i.e., listed above as items i) and ii)), and it is the reason for the frequency of their occurrences being different.
C1 [Wu, Chin-Chun] USN, Res Lab, Washington, DC 20375 USA.
[Lepping, R. P.] NASA GSFC, Greenbelt, MD 20771 USA.
RP Wu, CC (reprint author), USN, Res Lab, 4555 Overlook Ave, Washington, DC 20375 USA.
EM Chin-Chun.Wu@NRL.Navy.mil; Ronald.P.Lepping@gmail.com
FU NASA [NNH09AM46I]
FX We wish to thank the team at Kyoto University, Kyoto, Japan for
providing the Dst data, and the NSSDC at Goddard Space Flight
Center/NASA for providing Wind and ACE data. This work was supported by
the NASA "Living With a Star Targeted Research and Technology program"
under grant number NNH09AM46I.
NR 40
TC 22
Z9 22
U1 1
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD MAR
PY 2011
VL 269
IS 1
BP 141
EP 153
DI 10.1007/s11207-010-9684-3
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 738FZ
UT WOS:000288626700010
ER
PT J
AU Bodson, M
Frost, SA
AF Bodson, Marc
Frost, Susan A.
TI Load Balancing in Control Allocation
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
ID REENTRY VEHICLES; ALGORITHM
AB Next-generation aircraft with a large number of actuators will require advanced control allocation methods to compute the actuator commands needed to follow desired trajectories while respecting system constraints. Previously, algorithms were proposed to minimize the l(1) or l(2) norms of the tracking error and of the actuator deflections. This paper discusses the alternative choice of the l(infinity) norm, or the sup norm. Minimization of the control effort translates into the minimization of the maximum actuator deflection (min-max optimization). This paper shows how the problem can be solved effectively by converting it into a linear program and solving it using a simplex algorithm. Properties of the algorithm are also investigated through examples. In particular, the min-max criterion results in a type of load balancing, where the load is the desired command and the algorithm balances this load among various actuators. The solution using the l(infinity) norm also results in better robustness to failures and lower sensitivity to nonlinearities in illustrative examples. This paper also discusses the extension of the results to a normalized l(infinity) norm, where the norm of the actuator deflections are scaled by the actuator limits. Minimization of the control effort then translates into the minimization of the maximum actuator deflection as a percentage of its range of motion.
C1 [Bodson, Marc] Univ Utah, Elect & Comp Engn Dept, Salt Lake City, UT 84112 USA.
[Frost, Susan A.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Bodson, M (reprint author), Univ Utah, Elect & Comp Engn Dept, 50 S Cent Campus Dr,Room 3280, Salt Lake City, UT 84112 USA.
NR 31
TC 9
Z9 12
U1 0
U2 2
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 MAR-APR
PY 2011
VL 34
IS 2
BP 380
EP 387
DI 10.2514/1.51952
PG 8
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 735JA
UT WOS:000288409000005
ER
PT J
AU Tang, HB
Robinson, JE
Denery, DG
AF Tang, Huabin
Robinson, John E.
Denery, Dallas G.
TI Tactical Conflict Detection in Terminal Airspace
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
AB Air traffic systems have long relied on automated short-term conflict prediction algorithms to warn controllers of impending conflicts (losses of separation). The complexity of terminal airspace has proven difficult for such systems, as it often leads to excessive false alerts. Thus, the legacy system, called Conflict Alert, which currently provides short-term alerts in both en route and terminal airspace, is often inhibited or desensitized in areas where frequent false alerts occur, even though the alerts are provided only when an aircraft is in dangerous proximity of other aircraft. This research investigates how a minimal level of flight-intent information may be used to improve short-term conflict detection in terminal airspace such that it can be used by the controller to maintain legal aircraft separation. The flight-intent information includes a site-specific nominal arrival route and inferred altitude clearances in addition to the flight plan that includes the area-navigation departure route. A new tactical conflict detection algorithm is proposed, which uses a single analytic trajectory, determined from the flight intent and the current state information of the aircraft, and includes a complex set of current, dynamic separation standards for terminal airspace. The new algorithm is compared with an algorithm that models a known en route algorithm and another algorithm that models Conflict Alert. This is done by analysis of false-alert rate and alert lead time with the use of recent real-world data of arrival and departure operations and a large set of operational error cases from the Dallas/Fort Worth terminal radar approach control. The new algorithm yielded a false-alert rate of two per hour and an average alert lead time of 38 s.
C1 [Tang, Huabin; Robinson, John E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Denery, Dallas G.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
RP Tang, HB (reprint author), NASA, Ames Res Ctr, AFT 210-6, Moffett Field, CA 94035 USA.
EM huabin.tang-1@nasa.gov; john.e.robinson@nasa.gov; ddenery@ucsc.edu
NR 20
TC 6
Z9 6
U1 1
U2 8
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 MAR-APR
PY 2011
VL 34
IS 2
BP 403
EP 413
DI 10.2514/1.51898
PG 11
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 735JA
UT WOS:000288409000007
ER
PT J
AU Park, M
Przekop, A
Phairoh, T
Huang, JK
Mei, C
AF Park, Minseock
Przekop, Adam
Phairoh, Thongchai
Huang, Jen-Kuang
Mei, Chuh
TI Adaptive Control of Nonlinear Free Vibration of Shallow Shell Using
Piezoelectric Actuators
SO AIAA JOURNAL
LA English
DT Article
ID COMPOSITE PLATES; ACTIVE CONTROL; PANEL FLUTTER; ELEMENT
AB A coupled structural-electrical nonlinear modal finite-element multiple-mode formulation for laminated composite shallow shells with embedded piezoelectric sensors and actuators is presented for the suppression of large-amplitude undamped free vibrations. Composite shells exhibiting both softening and hardening behavior are investigated. The linear quadratic regulator combined with an extended Kalman filter is employed as an active controller for the suppression of nonlinear free vibrations. However, when the frequency of limit-cycle oscillations is suddenly changed from the softening to the hardening response characteristics or vice versa, active controller has difficulties to adjust the control parameters to cope with the changed structural response. To mitigate this issue, the currently developed controller is adaptively designed using the system identification which has the ability to identify the frequency of limit-cycle oscillations. It is shown that the adaptive controller constructed of the linear quadratic regulator and extended Kalman filter with system identification is suitable for suppression of the sudden change of shallow-shell response characteristics. The norm of optimal feedback control gain method for actuators and the norm of Kalman filter estimator gain method for sensors are employed to determine their optimal locations, respectively. Two different self-sensing actuator types, PZT5A and macrofiber composite, are used and their control performance for the suppression of the oscillations is compared. The numerical results illustrate that the adaptive controller can successfully suppress the nonlinear free vibrations, even with unknown sudden changes in the multimode response characteristic.
C1 [Park, Minseock; Huang, Jen-Kuang; Mei, Chuh] Old Dominion Univ, Dept Mech & Aerosp Engn, Norfolk, VA 23529 USA.
[Przekop, Adam] Analyt Serv & Mat Inc, NASA Langley Res Ctr, Hampton, VA 23666 USA.
[Phairoh, Thongchai] Virginia State Univ, Dept Engn & Technol, Petersburg, VA 23806 USA.
RP Park, M (reprint author), Korean Air, MUAV Dev Ctr, Aircraft Dev Team, 461-1 Jeonmin Dong, Taejon 305811, South Korea.
EM mseockpark@koreanair.com; Adam.Przekop@nasa.gov; tphairoh@vsu.edu;
jhuang@odu.edu; cmei@odu.edu
NR 31
TC 4
Z9 4
U1 1
U2 12
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 MAR
PY 2011
VL 49
IS 3
BP 472
EP 488
DI 10.2514/1.38520
PG 17
WC Engineering, Aerospace
SC Engineering
GA 730UC
UT WOS:000288059200003
ER
PT J
AU Li, F
Choudhari, M
Chang, CL
Streett, C
Carpenter, M
AF Li, Fei
Choudhari, Meelan
Chang, Chau-Lyan
Streett, Craig
Carpenter, Mark
TI Computational Modeling of Roughness-Based Laminar Flow Control on a
Subsonic Swept Wing
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT AIAA 27th Applied Aerodynamics Conference
CY JUN 22-25, 2009
CL San Antonio, TX
SP Amer Inst Aeronaut & Astronaut
ID SECONDARY INSTABILITY; BOUNDARY-LAYER; VORTICES; TRANSITION
AB A combination of parabolized stability equations and secondary instability theory has been applied to a low-speed swept airfoil model with a chord Reynolds number of 7.15 million, with the goal of evaluating this methodology in the context of transition prediction for a known configuration for which roughness-based crossflow transition control has been demonstrated under flight conditions. Nonlinear parabolized stability equations computations indicate that progressive reduction in the growth of the linearly most amplified stationary crossflow mode can be achieved via increasingly stronger control input corresponding to the first harmonic of the target mode. The reduction in the target mode amplitude is accompanied by reduced linear growth rates of the high-frequency secondary instabilities that lead to rapid breakdown of the laminar flow. The secondary instability predictions based on secondary instability theory are shown to agree well with those based on the parabolized stability equations. The possibility of overcontrol is also assessed, and it is found that premature transition due to excessive control can be avoided by keeping the control amplitude below a certain threshold. The nonlinear development of the most unstable Z-mode secondary instability is traced using the parabolized stability equation method, so as to yield physics-based prediction of crossflow-dominated transition.
C1 [Li, Fei; Choudhari, Meelan; Chang, Chau-Lyan; Streett, Craig; Carpenter, Mark] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
RP Li, F (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
RI Choudhari, Meelan/F-6080-2017
OI Choudhari, Meelan/0000-0001-9120-7362
NR 24
TC 7
Z9 8
U1 0
U2 5
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 MAR
PY 2011
VL 49
IS 3
BP 520
EP 529
DI 10.2514/1.J050503
PG 10
WC Engineering, Aerospace
SC Engineering
GA 730UC
UT WOS:000288059200007
ER
PT J
AU Kulisch, U
Snyder, V
AF Kulisch, Ulrich
Snyder, Van
TI The exact dot product as basic tool for long interval arithmetic
SO COMPUTING
LA English
DT Article
DE Computer arithmetic; Arithmetic standard; Exact Dot Product;
Floating-point arithmetic; Scientific Computing
AB Computing with guarantees is based on two arithmetical features. One is fixed (double) precision interval arithmetic. The other one is dynamic precision interval arithmetic, here also called long interval arithmetic. The basic tool to achieve high speed dynamic precision arithmetic for real and interval data is an exact multiply and accumulate operation and with it an exact dot product. Pipelining allows to compute it at the same high speed as vector operations on conventional vector processors. Long interval arithmetic fully benefits from such high speed. Exactitude brings very high accuracy, and thereby stability into computation. This document, which has been incorporated into the draft standard for interval arithmetic being developed by IEEE P1788, specifies the implementation of an exact multiply and accumulate operation.
C1 [Kulisch, Ulrich] Univ Karlsruhe, Inst Angew & Numer Math, D-76128 Karlsruhe, Germany.
[Snyder, Van] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kulisch, U (reprint author), Univ Karlsruhe, Inst Angew & Numer Math, Englerstr 2, D-76128 Karlsruhe, Germany.
EM Ulrich.Kulisch@math.uka.de; Van.Snyder@jpl.nasa.gov
FU Institut fur Angewandte und Numerische Mathematik, Universitat
Karlsruhe; NASA at Jet Propulsion Laboratory, California Institute of
Technology
FX Part of this work supported by Institut fur Angewandte und Numerische
Mathematik, Universitat Karlsruhe.; Part of this work supported by NASA
at Jet Propulsion Laboratory, California Institute of Technology.
NR 12
TC 5
Z9 5
U1 0
U2 1
PU SPRINGER WIEN
PI WIEN
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA
SN 0010-485X
EI 1436-5057
J9 COMPUTING
JI Computing
PD MAR
PY 2011
VL 91
IS 3
BP 307
EP 313
DI 10.1007/s00607-010-0127-7
PG 7
WC Computer Science, Theory & Methods
SC Computer Science
GA 732FF
UT WOS:000288169700005
ER
PT J
AU Carozza, DA
Mysak, LA
Schmidt, GA
AF Carozza, David A.
Mysak, Lawrence A.
Schmidt, Gavin A.
TI Methane and environmental change during the Paleocene-Eocene thermal
maximum (PETM): Modeling the PETM onset as a two-stage event
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID CARBON-ISOTOPE EXCURSION; DISSOCIATION; HYDRATE; GAS; DIOXIDE; RELEASE;
FUEL
AB Anatmospheric CH4 box model coupled to a global carbon cycle box model is used to constrain the carbon emission associated with the PETM and assess the role of CH4 during this event. A range of atmospheric and oceanic emission scenarios representing different amounts, rates, and isotopic signatures of emitted carbon are used to model the PETM onset. The first 3 kyr of the onset, a pre-isotope excursion stage, is simulated by the atmospheric release of 900 to 1100 Pg C CH4 with a delta C-13 of -22 to -30 parts per thousand. For a global average warming of 3 degrees C, a release of CO2 to the ocean and CH4 to the atmosphere totalling 900 to 1400 Pg C, with a delta C-13 of -50 to -60 parts per thousand, simulates the subsequent 1-kyr isotope excursion stage. To explain the observations, the carbon must have been released over at most 500 years. The first stage results cannot be associated with any known PETM hypothesis. However, the second stage results are consistent with a methane hydrate source. More than a single source of carbon is required to explain the PETM onset. Citation: Carozza, D. A., L. A. Mysak, and G. A. Schmidt (2011), Methane and environmental change during the Paleocene-Eocene thermal maximum (PETM): Modeling the PETM onset as a two-stage event, Geophys. Res. Lett., 38, L05702, doi:10.1029/2010GL046038.
C1 [Carozza, David A.; Mysak, Lawrence A.] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ H3A 2K6, Canada.
[Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Carozza, DA (reprint author), McGill Univ, Dept Earth & Planetary Sci, 3450 Univ St, Montreal, PQ H3A 2A7, Canada.
EM david.carozza@mcgill.ca
RI Schmidt, Gavin/D-4427-2012;
OI Schmidt, Gavin/0000-0002-2258-0486; Carozza, David
Anthony/0000-0001-7343-9442
FU Hydro-Quebec; NSERC; FQRNT; Birks Family Foundation
FX The authors are grateful to J.F. Kasting for providing the
Walker-Kasting carbon cycle box model code and to two reviewers for
their insightful comments. This work was supported by scholarships
awarded to DAC from Hydro-Quebec, NSERC, FQRNT, and the Birks Family
Foundation. This work was also supported by an NSERC Discovery Grant
awarded to LAM.
NR 20
TC 8
Z9 8
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 MAR 1
PY 2011
VL 38
AR L05702
DI 10.1029/2010GL046038
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 731DM
UT WOS:000288086500001
ER
PT J
AU Langley, K
Kohler, J
Matsuoka, K
Sinisalo, A
Scambos, T
Neumann, T
Muto, A
Winther, JG
Albert, M
AF Langley, K.
Kohler, J.
Matsuoka, K.
Sinisalo, A.
Scambos, T.
Neumann, T.
Muto, A.
Winther, J. -G.
Albert, M.
TI Recovery Lakes, East Antarctica: Radar assessment of sub-glacial water
extent
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID WEST ANTARCTICA; ICE STREAMS; SIPLE DOME
AB A fast-flowing tributary of Recovery ice stream penetrates more than 500 km into the interior of East Antarctica. Recent satellite-based studies found surface features in the onset area of this tributary that indicate a significant subglacial hydraulic system, including four large smooth basins, the typical surface expression of large subglacial lakes, as well as eleven smaller areas over which ice-sheet surface elevations rapidly changed by discharge/filling of subglacial water. Here we present the first ice-penetrating radar evidence of subglacial conditions in this area. We identified a distinct ice-water interface only over a limited area within the boundaries of the investigated large smooth basins, previously hypothesized to be water-filled lakes. The radar characteristics in some areas are similar to those of a drained lake, indicating that parts of the bed are wet, but not a typical lake. We also find evidence for discrete water bodies outside of the lake boundaries. The lines of evidence indicate that the northern most two Recovery Lakes have recently drained. Citation: Langley, K., J. Kohler, K. Matsuoka, A. Sinisalo, T. Scambos, T. Neumann, A. Muto, J.-G. Winther, and M. Albert (2011), Recovery Lakes, East Antarctica: Radar assessment of sub-glacial water extent, Geophys. Res. Lett., 38, L05501, doi:10.1029/2010GL046094.
C1 [Langley, K.; Kohler, J.; Matsuoka, K.; Winther, J. -G.] Norwegian Polar Res Inst, N-9296 Tromso, Norway.
[Langley, K.] Univ Tromso, Dept Phys & Technol, Tromso, Norway.
[Sinisalo, A.] Univ Oslo, Dept Geosci, N-0316 Oslo, Norway.
[Scambos, T.; Muto, A.] Univ Colorado, CIRES, Natl Snow & Ice Data Ctr, Boulder, CO 80303 USA.
[Neumann, T.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
[Albert, M.] Dartmouth Coll, Thayer Sch Engn, Hanover, NH 03755 USA.
RP Langley, K (reprint author), Norwegian Polar Res Inst, N-9296 Tromso, Norway.
EM kirsty@npolar.no
RI Neumann, Thomas/D-5264-2012; Matsuoka, Kenichi/B-7298-2017;
OI Albert, Mary/0000-0001-7842-2359
FU Norwegian Polar Institute [152]; Research Council of Norway; National
Science Foundation of the USA
FX The authors would like to acknowledge all members of the Norwegian-US
IPY traverse. This work has been carried out under the umbrella of
ITASE-IDEA within the framework of IPY project number 152 funded by
Norwegian Polar Institute, the Research Council of Norway and the
National Science Foundation of the USA. This work is also a contribution
to ITASE. We thank Robin Bell, one anonymous reviewer, and the Editor
Eric Rignot for their constructive comments.
NR 20
TC 19
Z9 20
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 1
PY 2011
VL 38
AR L05501
DI 10.1029/2010GL046094
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 731DM
UT WOS:000288086500002
ER
PT J
AU Phlips, EJ
Badylak, S
Christman, M
Wolny, J
Brame, J
Garland, J
Hall, L
Hart, J
Landsberg, J
Lasi, M
Lockwood, J
Paperno, R
Scheidt, D
Staples, A
Steidinger, K
AF Phlips, Edward J.
Badylak, Susan
Christman, Mary
Wolny, Jennifer
Brame, Julie
Garland, Jay
Hall, Lauren
Hart, Jane
Landsberg, Jan
Lasi, Margaret
Lockwood, Jean
Paperno, Richard
Scheidt, Doug
Staples, Ariane
Steidinger, Karen
TI Scales of temporal and spatial variability in the distribution of
harmful algae species in the Indian River Lagoon, Florida, USA
SO HARMFUL ALGAE
LA English
DT Article
DE Dinoflagellates; Diatoms; Climate; Eutrophication; Pyrodinium
ID SAN-FRANCISCO BAY; PYRODINIUM-BAHAMENSE; PHYTOPLANKTON BLOOMS;
MARINE-PHYTOPLANKTON; RESOURCE COMPETITION; SEAGRASS DEPTH; PUFFER FISH;
COASTAL; WATERS; MODEL
AB This paper describes the results of a harmful algal bloom (HAB) monitoring effort in the Indian River Lagoon. The goal of the study was to describe spatial and temporal variability in the distribution, frequency of occurrence, and composition of HABs, along with an examination of potential driving factors, such as hydrologic conditions and nutrient concentrations. Six sampling sites in the northern lagoon were selected for the study. The composition and abundance of the phytoplankton community was determined microscopically. Water column parameters measured in the study included salinity, water temperature, Secchi depth, total phosphorus, and total nitrogen.
Dinoflagellates, diatoms or cyanobacteria dominated the phytoplankton communities in terms of biovolume at all six sampling sites. Five potential toxin producing species were observed at bloom levels during the study period, including the diatom Pseudo-nitzschia calliantha and the dinoflagellates Pyrodinium bahamense var. bahamense, Prorocentrum rathymum, Cochlodinium polykrikoides, and Karlodinium veneficum. The saxitoxin-producing dinoflagellate P. bahamense var. bahamense had the highest biovolume observed over the study period, 33.9 x 10(6) mu m(3) ml(-1), and was present in almost half of the samples collected. Three non-toxic HAB species were observed at bloom levels of biovolume, including Akashiwo sanguinea, Peridinium quinquecorne, and Kryptoperidinium foliaceum. As part of this study, a statistical approach to estimating the probability of detecting HAB events was explored, using three common and important HAB species in the IRL, P. bahamense var. bahamense, A. sanguinea and P. calliantha, as exemplars. The potential driving factors for HAB events are discussed within the context of the hydrological, meteorological and watershed characteristics of the lagoon. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Phlips, Edward J.; Badylak, Susan; Hart, Jane; Lockwood, Jean] Univ Florida, Dept Fisheries & Aquat Sci, Gainesville, FL 32653 USA.
[Christman, Mary] Univ Florida, Dept Stat, Gainesville, FL 32611 USA.
[Wolny, Jennifer; Steidinger, Karen] Florida Inst Oceanog, St Petersburg, FL 33701 USA.
[Garland, Jay; Scheidt, Doug] NASA, Dynamac Corp, Life Sci Serv Contract, Kennedy Space Ctr, FL 32899 USA.
[Hall, Lauren] St Johns River Water Management Dist, Palm Bay, FL 32909 USA.
[Brame, Julie; Landsberg, Jan] Fish & Wildlife Res Inst, Florida Fish & Wildlife & Conservat Commiss, St Petersburg, FL 33701 USA.
[Lasi, Margaret] St Johns River Water Management Dist, Palatka, FL 32178 USA.
[Paperno, Richard; Staples, Ariane] Fish & Wildlife Res Inst, Florida Wildlife & Conservat Commiss, Melbourne, FL 32901 USA.
RP Phlips, EJ (reprint author), Univ Florida, Dept Fisheries & Aquat Sci, 7922 NW 71st St, Gainesville, FL 32653 USA.
EM phlips@ufl.edu
OI Wolny, Jennifer L./0000-0002-3556-5015
FU St. Johns River Water Management District; U.S.E.P.A.
FX The authors thank Joey Chait, Phyllis Hansen, Heather Manley, Lance
Riley for their assistance in this study. Special thanks to the Florida
Wildlife and Fish Commission Law Enforcement Office in Titusville for
their logistical assistance in this study. The research was funded by
grants from the St. Johns River Water Management District and the
U.S.E.P.A. National Estuarine Program.[TS]
NR 72
TC 26
Z9 27
U1 7
U2 61
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1568-9883
J9 HARMFUL ALGAE
JI Harmful Algae
PD MAR
PY 2011
VL 10
IS 3
BP 277
EP 290
DI 10.1016/j.hal.2010.11.001
PG 14
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 733ZE
UT WOS:000288302200005
ER
PT J
AU Manning, CV
Ma, YJ
Brain, DA
McKay, CP
Zahnle, KJ
AF Manning, Curtis V.
Ma, Yingjuan
Brain, David A.
McKay, Christopher P.
Zahnle, Kevin J.
TI Parametric analysis of modeled ion escape from Mars
SO ICARUS
LA English
DT Article
DE Mars; Atmosphere; Solar wind
ID SOLAR-WIND INTERACTION; PLASMA ENVIRONMENT; EVOLUTION; WATER
AB We develop a parametric fit to the results of a detailed magnetohydrodynamic (MHD) study of the response of ion escape rates (O(+), O(2)(+) and CO(2)(+)) to strongly varied solar forcing factors, as a way to efficiently extend the MHD results to different conditions. We then use this to develop a second, evolutionary model of solar forced ion escape. We treat the escape fluxes of ion species at Mars as proportional to the product of power laws of four factors - that of the EUV flux R(euv), the solar wind particle density R(rho), its velocity (squared) R(nu 2), and the interplanetary magnetic field pressure R(B2), where forcing factors are expressed in units of the current epoch-averaged values. Our parametric model is: phi(i) = phi(0)(i)R(euv)(alpha(i))R(rho)(beta(i))R(nu 2)(gamma(i))R(B2)(delta(i)) where phi(i) is the escape flux of ion i. We base our study on the results of just six provided MHD model runs employing large forcing factor variations, and thus construct a successful, first-order parametric model of the MHD program. We perform a five-dimensional least squares fit of this power law model to the MHD results to derive the flux normalizations and the indices of the solar forcing factors. For O(+), we obtain the values, 1.73 x 10(24) s(-1), 0.782, 0.251, 0.382, and 0.214, for phi(0), alpha, beta, gamma, and delta, respectively. For O(2)(+), the corresponding values are 1.68 x 10(24) s(-1), -0.393, 0.798, 0.967, and 0.533. For CO(2)(+), they are 8.66 x 10(22) s(-1), -0.427, 1.083, 1.214, and 0.690. The fit reproduces the MHD results to an average error of about 5%, suggesting that the power laws are broadly representative of the MHD model results. Our analysis of the MHD model shows that by itself an increase in R(EUV) enhances O(+) loss, but suppresses the escape of O(2)(+) and CO. whereas increases in solar wind (i.e., in R(rho), R(nu 2) and R(B2), with R(euv), constant) favors the escape of heavier ions more than light ions. The ratios of escaping ions detectable at Mars today can be predicted by this parametric fit as a function of the solar forcing factors. We also use the parametric model to compute escape rates over martian history. This second parametric model expresses ion escape functions of one variable (per ion), phi(i) = phi(0)(i)(t/t(0))(-xi(i)) The xi(i) are linear combinations of the epoch-averaged ion escape sensitivities, which are seen to increase with ion mass. We integrate the CO(2)(+) and oxygen ion escape rates over time, and find that in the last 3.85 Gyr, Mars would have lost about 25(-0.19)(+85) mbars of CO(2)(+), and 0.64(-0.34)(+0.62) meters of water (from O(+) and O(2)(+)) from ion escape. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Manning, Curtis V.; Brain, David A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Manning, Curtis V.; McKay, Christopher P.; Zahnle, Kevin J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ma, Yingjuan] IGPP, Los Angeles, CA 90065 USA.
RP Manning, CV (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM cmanning@ssl.berkeley.edu
RI Ma, Yingjuan/B-4895-2017
OI Ma, Yingjuan/0000-0003-2584-7091
FU NASA [NNX10AB75A]
FX We acknowledge support from NASA Grant NNX10AB75A. We also thank the two
anonymous referees for their comments which led to important
improvements in our paper.
NR 28
TC 4
Z9 4
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2011
VL 212
IS 1
BP 131
EP 137
DI 10.1016/j.icarus.2010.11.028
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700010
ER
PT J
AU Fieber-Beyer, SK
Gaffey, MJ
Abell, PA
AF Fieber-Beyer, Sherry K.
Gaffey, Michael J.
Abell, Paul A.
TI Mineralogical characterization of near-Earth Asteroid (1036) Ganymed
SO ICARUS
LA English
DT Article
DE Asteroids; Near-Earth Objects; Asteroids, Composition; Infrared
observations; Mineralogy
ID MAIN-BELT; REFLECTANCE SPECTRA; SPECTROSCOPIC SURVEY; PORTALES VALLEY;
INFRARED PHOTOMETRY; ORDINARY CHONDRITE; METEORITE BRECCIA; SURFACE
MATERIALS; COLOR VARIATIONS; IRON-METEORITES
AB We present a mineralogical assessment of near-Earth Asteroid, (1036) Ganymed, using data obtained May 18, 2006 UT combined with 24 Color Asteroid Survey data to cover the spectral interval of 0.3-2.45 mu m. Results of the analysis indicate (1036) Ganymed is an S (VI) asteroid with a surface silicate assemblage consisting primarily of orthopyroxene, (Fs(23(+/- 5))Wo(3(+/- 3))), consistent with calculated band centers and band area ratios (BAR). (1036) Ganymed appears to be once part of a large mesosiderite containing howardite, eucrite, and diogenite (HED) pyroxenes mixed with metal that was broken apart and dispersed. The calculated composition of the average pyroxenes in the surface material of (1036) Ganymed is consistent with mesosiderite pyroxenes, in particular the diogenites. A second possibility could be (1036) Ganymed is not yet represented in the meteorite collection. Our investigation has confirmed Ganymed is not a parent body of the ordinary chondrites and is not genetically related to (433) Eros. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Fieber-Beyer, Sherry K.; Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
[Abell, Paul A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Fieber-Beyer, SK (reprint author), Univ N Dakota, Dept Space Studies, Univ Stop 9008, Grand Forks, ND 58202 USA.
EM sherryfieb@hotmail.com
FU NASA [NNG04GJ86G, NNX07AP73G, NNX07AL29G]; NASA NESSF [NNX08AW0414]
FX Various portions of this research were supported by NASA Planetary
Geology and Geophysics (PGG) Program Grants NNG04GJ86G and NNX07AP73G,
NASA Near Earth Objects Observations (NEOO) Program Grant NNX07AL29G,
and NASA NESSF Grant NNX08AW0414. SKF would like to thank Vishnu Reddy
for his help during the collection of data and his suggestions to
improve the manuscript.
NR 71
TC 6
Z9 6
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2011
VL 212
IS 1
BP 149
EP 157
DI 10.1016/j.icarus.2010.12.013
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700012
ER
PT J
AU Veeder, GJ
Davies, AG
Williams, DA
Matson, DL
Johnson, TV
Radebaugh, J
AF Veeder, Glenn J.
Davies, Ashley Gerard
Williams, David A.
Matson, Dennis L.
Johnson, Torrence V.
Radebaugh, Jani
TI Io: Heat flow from dark paterae
SO ICARUS
LA English
DT Article
DE Io; Volcanism; Jupiter, Satellites
ID INFRARED MAPPING SPECTROMETER; GALILEO NIMS DATA; JUPITERS MOON IO;
VOLCANIC ACTIVITY; HOT-SPOTS; PHOTOPOLARIMETER-RADIOMETER; GLOBAL
DISTRIBUTION; ACTIVE VOLCANISM; IMAGING DATA; MU-M
AB Dark paterae on the jovian satellite Io are evidence of recent volcanic activity. Some paterae appear to be entirely filled with dark volcanic material, while others have only partially darkened floors. Dark paterae have area and heat flow longitudinal distributions that are bimodal as well as anti-correlated with the longitudinal distribution of mountains on Io at a global scale. As part of our study of Io's total heat flow, we have examined the darkest paterae and quantified their thermal emission in order to assess their contribution. This is the first time that the areas of the dark material in these paterae have been measured with such precision and correlated with their thermal emission. Dark paterae yield a significantly larger contribution to Io's heat flow than dark volcanic fields. Dark paterae (including Loki Patera) yield at least similar to 4 x 10(13) W or similar to 40% of Io's total heat flow. In comparison, dark flow fields yield similar to 10(13) W or similar to 10% of Io's total heat flow. Of the total heat loss from dark paterae, Loki Patera alone yields similar to 10(13) W or similar to 10% of Io's total thermal emission. (C) 2011 Published by Elsevier Inc.
C1 [Veeder, Glenn J.; Davies, Ashley Gerard; Matson, Dennis L.; Johnson, Torrence V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Radebaugh, Jani] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ashley.Davies@jpl.nasa.gov
FU NASA
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract to NASA. G.J.V., A.G.D. and
D.L.M. are supported by grants from the NASA PGG and OPR programs.
NR 86
TC 17
Z9 17
U1 2
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2011
VL 212
IS 1
BP 236
EP 261
DI 10.1016/j.icarus.2010.09.026
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700019
ER
PT J
AU Black, GJ
Campbell, DB
Carter, LM
AF Black, G. J.
Campbell, D. B.
Carter, L. M.
TI Ground-based radar observations of Titan: 2000-2008
SO ICARUS
LA English
DT Article
DE Titan; Saturn, Satellites; Radar observations
ID CASSINI RADAR; GALILEAN SATELLITES; SURFACE-PROPERTIES; MICROWAVE;
LAKES; MARS; REFLECTIVITY; ATMOSPHERE; SCATTERING; GOLDSTONE
AB We have observed Titan with the Arecibo Observatory's 12.6 cm wavelength radar system during the last eight oppositions of the Saturn system with sufficient sensitivity to characterize its scattering properties as a function of sub-Earth longitude. In a few sessions the Green Bank Telescope was used as the receiving instrument in a bistatic configuration to boost sub-radar track length and integration time. Radar echo spectra have been obtained for a total of 92 viewing geometries with sub-Earth locations scattered through all longitudes and at latitudes between 7.6 degrees S and 26.3 degrees S, close to the maximum southern excursion of the sub-Earth track. We find Titan to have globally average radar albedos at this wavelength of 0.161 in the opposite circular polarization sense as that transmitted (OC) and 0.074 in the same sense (SC), giving a polarization ratio SC/OC of 0.46. These values are intermediate between lower reflectivity rocky surfaces and higher reflectivity clean icy surfaces. The variations with longitude in general mirror the surface brightness variations seen through the infrared atmospheric windows. Xanadu Regio's radar reflectivity and polarization ratio are higher than the global averages, and suggest that its composition is relatively cleaner water ice or, possibly, some other material with low propagation loss at radio wavelengths. For all echo spectra most of the power is in a broad diffuse component but with a specular component whose strength and narrowness is highly variable as a function of surface location. For all data we fit a sum of the standard Hagfors scattering law describing the specular component and an empirical diffuse radar scattering model to extract bulk parameters of the surface. Many areas exhibit very narrow specular reflections implying terrain that are quite flat on centimeter to meter scales over spans of tens to perhaps hundreds of kilometers. The proportion of spectra showing these narrow specular echoes has fallen significantly over the observational time span, indicating either a latitudinal effect related to terrain differences or changing surface conditions over the past several years. A few radar tracks, especially those from the 2008 session, overlap some high resolution Cassini RADAR imagery swaths to allow a direct comparison with terrain. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Black, G. J.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Campbell, D. B.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Carter, L. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Black, GJ (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
EM gblack@virginia.edu
RI Carter, Lynn/D-2937-2012
FU NASA
FX We acknowledge support from the NASA Planetary Astronomy Program (for
GJB) and the NASA Planetary Geology and Geophysics Program (for DBC).
The Arecibo Observatory is part of the National Astronomy and Ionosphere
Center, which is operated by Cornell University under a cooperative
agreement with the National Science Foundation. The Green Bank Telescope
is operated by the National Radio Astronomy Observatory, a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. Ephemerides essential for this work were
provided by John Chandler at the Smithsonian Institution and Jon
Giorgini at JPL. The staff at the Arecibo Observatory and Green Bank
Telescope contributed significantly to the success of the observations.
We appreciate the thorough reviews by Lauren Wye and an anonymous
reviewer that greatly improved the manuscript.
NR 57
TC 2
Z9 2
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2011
VL 212
IS 1
BP 300
EP 320
DI 10.1016/j.icarus.2010.10.025
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700024
ER
PT J
AU Janssen, MA
Le Gall, A
Wye, LC
AF Janssen, M. A.
Le Gall, A.
Wye, L. C.
TI Anomalous radar backscatter from Titan's surface?
SO ICARUS
LA English
DT Article
DE Titan; Satellites, Surfaces; Radio observations; Radar observations
ID GREENLAND ICE-SHEET; CASSINI RADAR; GALILEAN SATELLITES; COHERENT
BACKSCATTER; RADIOMETER; SAR
AB Since Cassini arrived at Saturn in 2004, its moon Titan has been thoroughly mapped by the RADAR instrument at 2-cm wavelength, in both active and passive modes. Some regions on Titan, including Xanadu and various bright hummocky bright terrains, contain surfaces that are among the most radar-bright encountered in the Solar System. This high brightness has been generally attributed to volume scattering processes in the inhomogeneous, low-loss medium expected for a cold, icy satellite surface. We can test this assumption now that the emissivity has been obtained from the concurrent radiometric measurements for nearly all the surface, with unprecedented accuracy (Janssen et al., and the Cassini RADAR Team [2009]. Icarus 200, 222-239). Kirchhoffs law of thermal radiation relates the radar and radiometric properties in a way that has never been fully exploited. In this paper we examine here how this law may be applied in this case to better understand the nature of Titan's radar-bright regions. We develop a quantitative model that, when compared to the observational data, allows us to conclude that either the reflective characteristics of the putative volume scattering subsurface must be highly constrained, or, more likely, organized structure on or in the surface is present that enhances the backscatter. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Janssen, M. A.; Le Gall, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wye, L. C.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
RP Janssen, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michael.a.janssen@jpl.nasa.gov; alice.le.-gall@jpl.nasa.gov;
lcwye@stanford.edu
FU National Aeronautics and Space Administration (NASA)
FX This research was conducted at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA). The authors wish to thank
R. West for discussions about the radar calibration, W. Smythe, H.
Zebker, J. van Zyl, E. Rignot, and S. Hensley for discussions on various
aspects of backscattering from surfaces, A. Hayes for his help with
ArcGIS, and two anonymous reviewers for their careful reviews and very
helpful comments. We also gratefully acknowledge those who designed,
developed and operate the Cassini/Huygens mission, which is a joint
endeavor of NASA, the European Space Agency (ESA), and the Italian Space
Agency (ASI) and is managed by JPL/Caltech under a contract with NASA.
NR 34
TC 14
Z9 14
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 MAR
PY 2011
VL 212
IS 1
BP 321
EP 328
DI 10.1016/j.icarus.2010.11.026
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700025
ER
PT J
AU Blackburn, DG
Buratti, BJ
Ulrich, R
AF Blackburn, David G.
Buratti, Bonnie J.
Ulrich, Richard
TI A bolometric Bond albedo map of Iapetus: Observations from Cassini VIMS
and ISS and Voyager ISS
SO ICARUS
LA English
DT Article
DE Iapetus; Photometry; Satellites, Surfaces
ID INFRARED MAPPING SPECTROMETER; DARK SIDE; IMAGING SCIENCE; PHOTOMETRY;
LAPETUS; ORIGIN; SATURN; SATELLITES; DICHOTOMY; SURFACE
AB We utilized Cassini VIMS, Cassini ISS, and Voyager ISS observations of Iapetus to produce the first bolometric Bond albedo map of Iapetus. The average albedo values for the leading and trailing hemispheres are 0.06 +/- 0.01 and 0.25 +/- 0.03, respectively. However, the bright material in high-resolution ISS images has a value of 0.38 +/- 0.04, highlighting the importance of resolution in determining accurate albedo values for Iapetus due to the speckling of localized regions of dark material into the trailing hemisphere. The practical application of this map is determining more accurate surface temperatures in thermal models; these albedo values translate into first order blackbody temperatures of 125.5 K and 118.4 K for the trailing and leading hemispheres at the semi-major axis. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Blackburn, David G.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA.
[Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ulrich, Richard] Univ Arkansas, Dept Chem Engn, Fayetteville, AR 72701 USA.
RP Blackburn, DG (reprint author), Univ Arkansas, Arkansas Ctr Space & Planetary Sci, 202 Old Museum Bldg, Fayetteville, AR 72701 USA.
EM dgblackb@uark.edu
FU National Aeronautics and Space Administration; University of Arkansas;
Arkansas Space Grant Consortium
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, and the University of Arkansas and
sponsored by the National Aeronautics and Space Administration's Space
Grant Program. We would like to thank the University of Arkansas and the
Arkansas Space Grant Consortium for support, as well as helpful
conversation with Mike Hicks, Ken Lawrence, Karly Pitman, and Edgard
Rivera-Valentin. We also appreciate the comments and suggestions of John
Spencer and an anonymous reviewer that improved the quality of our
manuscript.
NR 29
TC 5
Z9 5
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 MAR
PY 2011
VL 212
IS 1
BP 329
EP 338
DI 10.1016/j.icarus.2010.12.022
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700026
ER
PT J
AU Irwin, PGJ
Teanby, NA
Davis, GR
Fletcher, LN
Orton, GS
Tice, D
Kyffin, A
AF Irwin, P. G. J.
Teanby, N. A.
Davis, G. R.
Fletcher, L. N.
Orton, G. S.
Tice, D.
Kyffin, A.
TI Uranus' cloud structure and seasonal variability from Gemini-North and
UKIRT observations
SO ICARUS
LA English
DT Article
DE Atmospheres, Composition; Uranus; Uranus, Atmosphere; Atmospheres,
Dynamics; Data reduction techniques
ID INFRARED-ABSORPTION SPECTRA; RADIATIVE-TRANSFER; TEMPERATURES; DYNAMICS;
PAIRS; BAND; ATMOSPHERE; EQUINOX; 20-K
AB Observations of Uranus were made in September 2009 with the Gemini-North telescope in Hawaii, using both the NIES and NIRI instruments. Observations were acquired in Adaptive Optics mode and have a spatial resolution of approximately 0.1 ''.
NIRI images were recorded with three spectral filters to constrain the overall appearance of the planet: J, H-continuum and CH(4)(long), and long slit spectroscopy measurements were also made (1.49-1.79 mu m) with the entrance slit aligned on Uranus' central meridian. To acquire spectra from other points on the planet, the NIFS instrument was used and its 3 '' x 3 '' field of view stepped across Uranus' disc. These observations were combined to yield complete images of Uranus at 2040 wavelengths between 1.476 and 1.803 mu m.
The observed spectra along Uranus central meridian were analysed with the NEMESIS retrieval tool and used to infer the vertical/latitudinal variation in cloud optical depth. We find that the 2009 Gemini data perfectly complement our observations/conclusions from UKIRT/UIST observations made in 2006-2008 and show that the north polar zone at 45 degrees N has continued to steadily brighten while that at 45 S has continued to fade. The improved spatial resolution of the Gemini observations compared with the non-AO UKIRT/UIST data removes some of the earlier ambiguities with our previous analyses and shows that the opacity of clouds deeper than the 2-bar level does indeed diminish towards the poles and also reveals a darkening of the deeper cloud deck near the equator, perhaps coinciding with a region of subduction. We find that the clouds at 45 degrees N,S lie at slightly lower pressures than the clouds at more equatorial latitudes, which suggests that they might possibly be composed of a different condensate, presumably CH(4) ice, rather than H(2)S or NH(3) ice, which is assumed for the deeper cloud. In addition, analysis of the centre-to-limb curves of both the Gemini/NIFS and earlier UKIRT/UIST 1FU observations shows that the main cloud deck has a well-defined top, and also allows us to better constrain the particle scattering properties.
Overall, Uranus appeared to be less convectively active in 2009 than in the previous 3 years, which suggests that now the northern spring equinox (which occurred in 2007) is passed the atmosphere is settling back into the quiescent state seen by Voyager 2 in 1986. However, a number of discrete clouds were still observed, with one at 15 degrees N found to lie near the 500 mb level, while another at 30 degrees N, was seen to be much higher at near the 200 mb level. Such high clouds are assumed to be composed of CH(4) ice. (C) 2011 Elsevier Inc. All rights reserved,
C1 [Irwin, P. G. J.; Fletcher, L. N.; Tice, D.; Kyffin, A.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
[Teanby, N. A.] Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England.
[Davis, G. R.] Joint Astron Ctr, Hilo, HI 96720 USA.
[Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Irwin, PGJ (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
EM irwin@atm.ox.ac.uk
RI Fletcher, Leigh/D-6093-2011;
OI Fletcher, Leigh/0000-0001-5834-9588; Teanby,
Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X
FU United Kingdom Science and Technology Facilities Council
FX We are grateful to the United Kingdom Science and Technology Facilities
Council for funding this research and also to our support astronomers:
Richard McDermid (2009), Chad Trujillo (2009), Andy Adamson (2007,
2008), Watson Varricattu (2006), and also to Ilona Soechting in the UK
Gemini Office. The Gemini Observatory is operated by the Association of
Universities for Research in Astronomy. Inc., under a cooperative
agreement with the NSF on behalf of the Gemini partnership: the National
Science Foundation (United States), the Science and Technology
Facilities Council (United Kingdom), the National Research Council
(Canada), CONICYT (Chile), the Australian Research Council (Australia),
Ministerio da Ciencia e Tecnologia (Brazil) and Ministerio de Ciencia,
Tecnologia e Innovacion Productiva (Argentina). The United Kingdom
Infrared Telescope is operated by the Joint Astronomy Centre on behalf
of the Science and Technology Facilities Council of the UK.
NR 27
TC 10
Z9 10
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2011
VL 212
IS 1
BP 339
EP 350
DI 10.1016/j.icarus.2010.12.018
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700027
ER
PT J
AU LaMarche, CQ
Curtis, JS
Metzger, PT
AF LaMarche, Casey Q.
Curtis, Jennifer Sinclair
Metzger, Philip T.
TI Permeability of JSC-1A: A lunar soil simulant
SO ICARUS
LA English
DT Article
DE Moon; Moon, surface; Regoliths; Cratering; Ices
ID GAS-TRANSPORT; POROUS-MEDIA; ICE; SURFACE; MOON; SUBLIMATION;
ANTARCTICA; POROSITY; MERCURY; WATER
AB The permeability of lunar soil simulant, JSC-1A, is measured over a range of bulk densities from 1550 to 2000 kg m(-3). The corresponding viscous flow permeability is 1 x 10(-12) m(2) to 6.1 x 10(-12) m(2) for this bulk density range. Implications of these values on the contamination of regolith by rockets, on barrier/enhancement to bulk flow of ice, and on cratering are discussed. Although the particle size and shape distribution of the JSC-1A are extremely wide, the permeability measurements agree surprisingly well with the Carman-Kozeny equation. The results provide evidence that the Carman-Kozeny model could be applicable to other naturally occurring soils if effective soil properties are considered. (C) 2010 Elsevier Inc. All rights reserved.
C1 [LaMarche, Casey Q.; Curtis, Jennifer Sinclair] Univ Florida, Dept Chem Engn, Gainesville, FL 32611 USA.
[Metzger, Philip T.] NASA, Granular Mech & Surface Syst Lab, Kennedy Space Ctr, FL 32899 USA.
RP LaMarche, CQ (reprint author), Univ Florida, Dept Chem Engn, Room 227 CHE POB 116005, Gainesville, FL 32611 USA.
EM clamarche@che.ufl.edu
RI Metzger, Philip/R-3136-2016
OI Metzger, Philip/0000-0002-6871-5358
NR 34
TC 7
Z9 7
U1 0
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2011
VL 212
IS 1
BP 383
EP 389
DI 10.1016/j.icarus.2010.12.015
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700031
ER
PT J
AU Baer, J
Chesley, SR
Milani, A
AF Baer, James
Chesley, Steven R.
Milani, Andrea
TI Development of an observational error model
SO ICARUS
LA English
DT Article
DE Asteroids; Orbit determination; Celestial mechanics
AB In calculating the orbit of a minor planet with a least-squares algorithm, current practice is to assume that all observations of a given era have the same uncertainty, and that the errors in these observations are uncorrelated. These assumptions are unrealistic: and they lead to sub-optimal orbits.
Our objective is to develop and validate an observational error model that provides realistic estimates of the uncertainties and correlations in asteroid observations. When used to populate the covariance matrix of the least-squares algorithm, the resulting orbits are shown to more accurately and precisely represent asteroid trajectories. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Baer, James] James Cook Univ, Sch Engn & Phys Sci, Townsville, Qld 4811, Australia.
[Chesley, Steven R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Milani, Andrea] Univ Pisa, Dipartimento Matemat, I-56127 Pisa, Italy.
RP Baer, J (reprint author), James Cook Univ, Sch Engn & Phys Sci, Townsville, Qld 4811, Australia.
EM jimbaer1@earthlink.net; steve.chesley@jpl.nasa.gov
NR 5
TC 5
Z9 5
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 MAR
PY 2011
VL 212
IS 1
BP 438
EP 447
DI 10.1016/j.icarus.2010.11.031
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 732KL
UT WOS:000288183700036
ER
PT J
AU West, KE
Jablonski, MR
Warfield, B
Cecil, KS
James, M
Ayers, MA
Maida, J
Bowen, C
Sliney, DH
Rollag, MD
Hanifin, JP
Brainard, GC
AF West, Kathleen E.
Jablonski, Michael R.
Warfield, Benjamin
Cecil, Kate S.
James, Mary
Ayers, Melissa A.
Maida, James
Bowen, Charles
Sliney, David H.
Rollag, Mark D.
Hanifin, John P.
Brainard, George C.
TI Blue light from light-emitting diodes elicits a dose-dependent
suppression of melatonin in humans
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE pineal; light-emitting diode
ID SEASONAL AFFECTIVE-DISORDER; SHORT-WAVELENGTH LIGHT; HUMAN CIRCADIAN
SYSTEM; HIGH-SENSITIVITY; ACTION SPECTRUM; GANGLION-CELLS;
PHOTORECEPTORS; RHYTHMS; NIGHT; ROD
AB West KE, Jablonski MR, Warfield B, Cecil KS, James M, Ayers MA, Maida J, Bowen C, Sliney DH, Rollag MD, Hanifin JP, Brainard GC. Blue light from light-emitting diodes elicits a dose-dependent suppression of melatonin in humans. J Appl Physiol 110: 619-626, 2011. First published December 16, 2010; doi:10.1152/japplphysiol.01413.2009.-Light suppresses melatonin in humans, with the strongest response occurring in the short-wavelength portion of the spectrum between 446 and 477 nm that appears blue. Blue monochromatic light has also been shown to be more effective than longer-wavelength light for enhancing alertness. Disturbed circadian rhythms and sleep loss have been described as risk factors for astronauts and NASA ground control workers, as well as civilians. Such disturbances can result in impaired alertness and diminished performance. Prior to exposing subjects to short-wavelength light from light-emitting diodes (LEDs) (peak lambda = 469 nm; 1/2 peak bandwidth = 26 nm), the ocular safety exposure to the blue LED light was confirmed by an independent hazard analysis using the American Conference of Governmental Industrial Hygienists exposure limits. Subsequently, a fluence-response curve was developed for plasma melatonin suppression in healthy subjects (n = 8; mean age of 23.9 +/- 0.5 years) exposed to a range of irradiances of blue LED light. Subjects with freely reactive pupils were exposed to light between 2: 00 and 3: 30 AM. Blood samples were collected before and after light exposures and quantified for melatonin. The results demonstrate that increasing irradiances of narrowband blue-appearing light can elicit increasing plasma melatonin suppression in healthy subjects (P < 0.0001). The data were fit to a sigmoidal fluence-response curve (R(2) = 0.99; ED(50) = 14.19 mu W/cm(2)). A comparison of mean melatonin suppression with 40 mu W/cm(2) from 4,000 K broadband white fluorescent light, currently used in most general lighting fixtures, suggests that narrow bandwidth blue LED light may be stronger than 4,000 K white fluorescent light for suppressing melatonin.
C1 [West, Kathleen E.; Jablonski, Michael R.; Warfield, Benjamin; Cecil, Kate S.; James, Mary; Ayers, Melissa A.; Rollag, Mark D.; Hanifin, John P.; Brainard, George C.] Thomas Jefferson Univ, Dept Neurol, Philadelphia, PA 19107 USA.
[Maida, James; Bowen, Charles] NASA, Lyndon B Johnson Space Ctr, Habitabil & Human Factors Branch, Houston, TX 77058 USA.
[Sliney, David H.] USA, Environm Hyg Agcy, Aberdeen Proving Ground, Aberdeen, MD USA.
RP Brainard, GC (reprint author), Thomas Jefferson Univ, Dept Neurol, Philadelphia, PA 19107 USA.
EM george.brainard@jefferson.edu
FU National Space Biomedical Research Institute through NASA [NCC 9-58]
FX This work is supported by the National Space Biomedical Research
Institute through NASA NCC 9-58.
NR 61
TC 57
Z9 61
U1 4
U2 43
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 8750-7587
J9 J APPL PHYSIOL
JI J. Appl. Physiol.
PD MAR
PY 2011
VL 110
IS 3
BP 619
EP 626
DI 10.1152/japplphysiol.01413.2009
PG 8
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA 731RN
UT WOS:000288127100008
PM 21164152
ER
PT J
AU Thompson, AM
Allen, AL
Lee, S
Miller, SK
Witte, JC
AF Thompson, Anne M.
Allen, Amber L.
Lee, Sukyoung
Miller, Sonya K.
Witte, Jacquelyn C.
TI Gravity and Rossby wave signatures in the tropical troposphere and lower
stratosphere based on Southern Hemisphere Additional Ozonesondes
(SHADOZ), 1998-2007
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BREWER-DOBSON CIRCULATION; QUASI-BIENNIAL OSCILLATION; BIOMASS BURNING
EMISSIONS; EQUATORIAL KELVIN WAVES; OZONE CLIMATOLOGY; TROPOPAUSE LAYER;
WATER-VAPOR; SEASONAL EVOLUTION; BORNE OBSERVATIONS; DEEP CONVECTION
AB Prior investigations attempted to determine the relative influence of advection and convective processes on ozone and water vapor distributions in the tropical tropopause layer (TTL) through analyses of tracers, related physical parameters (e.g., outgoing long-wave radiation, precipitable water, and temperature), or with models. In this study, stable laminae in Southern Hemisphere Additional Ozonesonde Network (SHADOZ) ozone profiles from 1998 to 2007 are interpreted in terms of gravity waves (GW) or Rossby waves (RW) that are identified with vertical and quasi-horizontal displacements, respectively. Using the method of Pierce and Grant (1998) as applied by Thompson et al. (2007a, 2007b, 2010, 2011), amplitudes and frequencies in ozone laminae are compared among representative SHADOZ sites over Africa and the Pacific, Indian, and Atlantic oceans. GW signals maximize in the TTL and lower stratosphere. Depending on site and season, GW are identified in up to 90% of the soundings. GW are most prevalent over the Pacific and eastern Indian oceans, a distribution consistent with vertically propagating equatorial Kelvin waves. Ozone laminae from RW occur more often below the tropical tropopause and with lower frequency (< 20%). Gravity wave and Rossby wave indices (GWI, RWI) are formulated to facilitate analysis of interannual variability of wave signatures among sites. GWI is positively correlated with a standard ENSO (El Nino-Southern Oscillation) index over American Samoa (14 degrees S, 171 degrees W) and negatively correlated at Watukosek, Java (7.5 degrees S, 114 degrees E), Kuala Lumpur (3 degrees N, 102 degrees E), and Ascension Island (8 degrees S, 15 degrees W). Generally, the responses of GW and RW to ENSO are consistent with prior studies.
C1 [Thompson, Anne M.; Allen, Amber L.; Lee, Sukyoung; Miller, Sonya K.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Witte, Jacquelyn C.] SSAI, Lanham, MD USA.
[Witte, Jacquelyn C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thompson, AM (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
EM amt16@psu.edu; amber.allen@erg.com; sl@meteo.psu.edu;
smiller@meteo.psu.edu; jacquelyn.witte@nasa.gov
RI Thompson, Anne /C-3649-2014
OI Thompson, Anne /0000-0002-7829-0920
FU NASA [NNG05GP22G, NNX09AJ23G]
FX This research is based on the MS thesis of A. Loucks (Allen) and was
supported by NASA grants NNG05GP22G and NNX09AJ23G (thanks to M. J.
Kurylo and K. W. Jucks). We are grateful for comments by M. Fujiwara
(Hokkaido University), A. E. Dessler (Texas A&M University), J.-L.
Baray, and S. Venkataraman (Universite de la Reunion).
NR 108
TC 11
Z9 11
U1 1
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 1
PY 2011
VL 116
AR D05302
DI 10.1029/2009JD013429
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 731DW
UT WOS:000288087500001
ER
PT J
AU McGregor, SL
Hughes, WJ
Arge, CN
Owens, MJ
Odstrcil, D
AF McGregor, S. L.
Hughes, W. J.
Arge, C. N.
Owens, M. J.
Odstrcil, D.
TI The distribution of solar wind speeds during solar minimum: Calibration
for numerical solar wind modeling constraints on the source of the slow
solar wind
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MAGNETIC-FIELDS; CORONAL HOLES; ACCELERATION; FLUX; SUN
AB It took the solar polar passage of Ulysses in the early 1990s to establish the global structure of the solar wind speed during solar minimum. However, it remains unclear if the solar wind is composed of two distinct populations of solar wind from different sources (e.g., closed loops which open up to produce the slow solar wind) or if the fast and slow solar wind rely on the superradial expansion of the magnetic field to account for the observed solar wind speed variation. We investigate the solar wind in the inner corona using the Wang-Sheeley-Arge (WSA) coronal model incorporating a new empirical magnetic topology-velocity relationship calibrated for use at 0.1 AU. In this study the empirical solar wind speed relationship was determined by using Helios perihelion observations, along with results from Riley et al. (2003) and Schwadron et al. (2005) as constraints. The new relationship was tested by using it to drive the ENLIL 3-D MHD solar wind model and obtain solar wind parameters at Earth (1.0 AU) and Ulysses (1.4 AU). The improvements in speed, its variability, and the occurrence of high-speed enhancements provide confidence that the new velocity relationship better determines the solar wind speed in the outer corona (0.1 AU). An analysis of this improved velocity field within the WSA model suggests the existence of two distinct mechanisms of the solar wind generation, one for fast and one for slow solar wind, implying that a combination of present theories may be necessary to explain solar wind observations.
C1 [McGregor, S. L.; Hughes, W. J.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Arge, C. N.] Kirtland AFB, Albuquerque, NM 87117 USA.
[Odstrcil, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Owens, M. J.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
RP McGregor, SL (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
EM slmic@bu.edu
RI Owens, Mathew/B-3006-2010
OI Owens, Mathew/0000-0003-2061-2453
FU STC, National Science Foundation [ATM-0120950]
FX This work was supported by the Center for Integrated Space Weather
Modeling, which is funded by the STC program of the National Science
Foundation under Cooperative Agreement ATM-0120950. The OMNI data were
obtained from the Goddard Space Flight Center(GSFC)-SPDF OMNIWeb
interface at http://omniweb.gsfc.nasa.gov. The authors would also like
to acknowledge H. Rosenbauer (PI) and R. Schwenn for Helios 1 plasma
data, NSSDC, and GSFC-SPDF.
NR 31
TC 21
Z9 23
U1 0
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 MAR 1
PY 2011
VL 116
AR A03101
DI 10.1029/2010JA015881
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 731CM
UT WOS:000288083900001
ER
PT J
AU Sehirlioglu, A
Sayir, A
Dynys, F
Nittala, K
Jones, J
AF Sehirlioglu, Alp
Sayir, Ali
Dynys, Fred
Nittala, Krishna
Jones, Jacob
TI Structure and Piezoelectric Properties Near the Bismuth Scandium
Oxide-Lead Zirconate-Lead Titanate Ternary Morphotropic Phase Boundary
SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY
LA English
DT Article
ID SINGLE-CRYSTALS; SOLID-SOLUTION; CERAMICS; (1-X)BISCO3-XPBTIO(3);
MICROSTRUCTURE; SYSTEM
AB Ternary phase diagram of BiScO3 (BS), PbZrO3 (PZ), and PbTiO3 (PT) was explored for identification of high-performance piezoelectrics for actuator applications. The ternary morphotropic phase boundary (MPB) connecting the binary MPBs of BS-PT (45/65) and PZ-PT (52/48) was determined using X-ray diffraction (XRD). High-temperature XRD and dielectric measurements were used to determine the phase transformation temperatures. Curie temperature (T-C) had a near linear dependence on composition, rate of which is determined for each component of the ternary independently. Specimens on the tetragonal side of the MPB exhibited lower high field resistivity and proper poling was not possible. Specimens on the rhombohedral side were superior with saturated hysteresis loops and piezoelectric coefficient (d(33))> 400 pm/V. Unlike phase transformation temperatures, the proximity to MPB was more dominant than the compositional effects in determining electrical and electromechanical properties, which maximized for the compositions closest to the MPB. Both weak- and high field properties are reported as a function of temperature.
C1 [Sehirlioglu, Alp; Sayir, Ali; Dynys, Fred] NASA, John Glenn Res Ctr, Cleveland, OH 44135 USA.
[Sehirlioglu, Alp; Sayir, Ali] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA.
[Nittala, Krishna; Jones, Jacob] Univ Florida, Dept Mat Sci & Engn, Gainesville, FL 32611 USA.
RP Sehirlioglu, A (reprint author), NASA, John Glenn Res Ctr, Cleveland, OH 44135 USA.
EM alp.sehirlioglu@case.edu
RI Jones, Jacob/A-8361-2008; Nittala, Krishna/F-5332-2012
FU Air Force Office of Scientific Research [FA 9550-06-1-0260]; U. S.
National Science Foundation [DMR-0746902]; U. S. Department of the Army
[W911NF-09-1-0435]
FX This work was financially supported by the Air Force Office of
Scientific Research Grant FA 9550-06-1-0260. Presented at 2009 U. S.
Navy Workshop on Acoustic Transduction Materials and Devices, State
College, PA, May 12-15, 2009 (Ceramics and Losses Session).; J. L. J.
acknowledges support from the U. S. National Science Foundation under
award DMR-0746902 and the U. S. Department of the Army under award
W911NF-09-1-0435.
NR 21
TC 9
Z9 9
U1 1
U2 20
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-7820
EI 1551-2916
J9 J AM CERAM SOC
JI J. Am. Ceram. Soc.
PD MAR
PY 2011
VL 94
IS 3
BP 788
EP 795
DI 10.1111/j.1551-2916.2010.04142.x
PG 8
WC Materials Science, Ceramics
SC Materials Science
GA 733KL
UT WOS:000288261500029
ER
PT J
AU Fischer, DG
Frazin, RA
Asipauskas, M
Carney, PS
AF Fischer, David G.
Frazin, Richard A.
Asipauskas, Marius
Carney, P. Scott
TI Information content of the near field: three-dimensional samples
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND
VISION
LA English
DT Article
ID INTERNAL-REFLECTION TOMOGRAPHY; BORN SCATTERED FIELDS;
IMAGE-RECONSTRUCTION; DIGITAL HOLOGRAPHY; INVERSE SCATTERING; DEPTH
RESOLUTION; FRESNEL ZONE; MICROSCOPY; SUPERRESOLUTION; OPTICS
AB We present an analysis of the accuracy and information content of three-dimensional reconstructions of the dielectric susceptibility of a sample from noisy, near-field holographic measurements, such as those made in scanning probe microscopy. Holographic measurements are related to the dielectric susceptibility via a linear operator within the accuracy of the first Born approximation. The maximum-likelihood reconstruction of the dielectric susceptibility is expressed as a linear combination of basis functions determined by singular value decomposition of the weighted measurement operator. Maximum a posteriori estimates based on prior information are also discussed. Semianalytical expressions are given for the likely error due to measurement noise in the basis function coefficients, resulting in effective resolution limits in all three dimensions. These results are illustrated by numerical examples. (C) 2011 Optical Society of America
C1 [Fischer, David G.] NASA, Glenn Res Ctr, Res & Technol Directorate, Cleveland, OH 44135 USA.
[Frazin, Richard A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Asipauskas, Marius] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
[Carney, P. Scott] Univ Illinois, Dept Elect & Comp Engn, Urbana, IL 61801 USA.
RP Fischer, DG (reprint author), NASA, Glenn Res Ctr, Res & Technol Directorate, Cleveland, OH 44135 USA.
EM dgfischer@nasa.gov
RI Frazin, Richard/J-2625-2012
FU United States Air Force Multidisciplinary Research Initiative
[F49620-03-1-0379]; National Aeronautics and Space Administration (NASA)
[NAG3-2764]
FX We would like to thank John C. Schotland, Brian J. Williams, and Farzad
Kamalabadi for useful discussions, P. S. Carney would like to
acknowledge support under United States Air Force Multidisciplinary
Research Initiative grant F49620-03-1-0379 and National Aeronautics and
Space Administration (NASA) grant NAG3-2764.
NR 38
TC 2
Z9 2
U1 0
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1084-7529
J9 J OPT SOC AM A
JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis.
PD MAR
PY 2011
VL 28
IS 3
BP 296
EP 306
DI 10.1364/JOSAA.28.000296
PG 11
WC Optics
SC Optics
GA 730DI
UT WOS:000288012400002
PM 21383809
ER
PT J
AU Khaykovich, B
Gubarev, MV
Bagdasarova, Y
Ramsey, BD
Moncton, DE
AF Khaykovich, B.
Gubarev, M. V.
Bagdasarova, Y.
Ramsey, B. D.
Moncton, D. E.
TI From x-ray telescopes to neutron scattering: Using axisymmetric mirrors
to focus a neutron beam
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
ID OPTICS; RADIOGRAPHY; DESIGN; LENS
AB We demonstrate neutron beam focusing by axisymmetric mirror systems based on a pair of mirrors consisting of a confocal ellipsoid and hyperboloid. Such a system, known as a Wolter mirror configuration, is commonly used in X-ray telescopes. The axisymmetric Wolter geometry allows nesting of several mirror pairs to increase collection efficiency. We implemented a system containing four nested Ni mirror pairs, which was tested by the focusing of a polychromatic neutron beam at the MIT Reactor. In addition, we have carried out extensive ray-tracing simulations of the mirrors and their performance in different situations. The major advantages of the Wolter mirrors are nesting for large angular collection and aberration-free performance. We discuss how these advantages can be utilized to benefit various neutron scattering methods, such as imaging, SANS, and time-of-flight spectroscopy. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Khaykovich, B.; Moncton, D. E.] 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.
[Bagdasarova, Y.; 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
OI Khaykovich, Boris/0000-0002-9490-2771
FU US Department of Energy, Office of Basic Energy Sciences
[DE-FG02-09ER46556, DE-FG02-09ER46557]; National Science Foundation
[DMR-0526754]
FX This research was supported by the US Department of Energy, Office of
Basic Energy Sciences, 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 25
TC 18
Z9 18
U1 1
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD MAR 1
PY 2011
VL 631
IS 1
BP 98
EP 104
DI 10.1016/j.nima.2010.11.110
PG 7
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 730OA
UT WOS:000288042100015
ER
PT J
AU Popescu, SC
Nelson, RF
AF Popescu, Sorin C.
Nelson, Ross F.
TI Special Issue - Lidar Remote Sensing for Characterizing Forest
Vegetation FOREWORD
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Editorial Material
C1 [Popescu, Sorin C.] Texas A&M Univ, Dept Ecosyst Sci & Management, College Stn, TX 77843 USA.
[Nelson, Ross F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Popescu, SC (reprint author), Texas A&M Univ, Dept Ecosyst Sci & Management, College Stn, TX 77843 USA.
RI Popescu, Sorin/D-5981-2015; Nelson, Ross/H-8266-2014
OI Popescu, Sorin/0000-0002-8155-8801;
NR 0
TC 1
Z9 1
U1 0
U2 4
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD MAR
PY 2011
VL 77
IS 3
SI SI
BP 217
EP 218
PG 2
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA 730RO
UT WOS:000288052100004
ER
PT J
AU Ghose, S
Cano, RJ
Britton, SM
Watson, KA
Jensen, BJ
Connell, JW
AF Ghose, S.
Cano, R. J.
Britton, S. M.
Watson, K. A.
Jensen, B. J.
Connell, J. W.
TI High Temperature VARTM of Phenylethynyl Terminated Imide (PETI) Resins
SO SAMPE JOURNAL
LA English
DT Article
ID COMPOSITES
AB Fabrication of composite structures using vacuum assisted resin transfer molding (VARTM) is generally more affordable than conventional autoclave techniques. Recent efforts have focused on adapting VARTM for the fabrication of high temperature composites. Due to their low melt viscosity and long melt stability, certain phenylethynyl terminated imides (PETI) can be processed into composites using high temperature VARTM (HT-VARTM). However, one of the disadvantages of the current HT-VARTM resin systems has been the high porosity of the resultant composites. For aerospace applications a void fraction of less than 2% is desired. In the current study, two PET! resins, LARC (TM) PETI-330 and LARC (TM) PETI-8 have been used to fabricate test specimens using HT-VARTM. The resins were infused into carbon fiber preforms at 260 degrees C and cured between 316 degrees C and 371 degrees C. Modifications to the thermal cycle used in the laminate fabrication have reduced the void content significantly (typically <= 3%) for carbon fiber biaxially woven fabric. Photomicrographs of the panels were taken and void contents were determined by acid digestion. For carbon fiber uniaxial fabric, void contents of less than 2% have been obtained using both PETI-8 and PETI-330. Mechanical properties of the panels were determined at both room and elevated temperatures. These include short beam shear and flexure tests. The results of this work are presented herein.
C1 [Ghose, S.; Watson, K. A.] Natl Inst Aerosp, Hampton, VA USA.
[Cano, R. J.; Britton, S. M.; Jensen, B. J.; Connell, J. W.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Ghose, S (reprint author), Natl Inst Aerosp, Hampton, VA USA.
EM sayata.ghose-1@nasa.gov
NR 16
TC 0
Z9 0
U1 2
U2 9
PU SAMPE PUBLISHERS
PI COVINA
PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA
SN 0091-1062
J9 SAMPE J
JI Sampe J.
PD MAR-APR
PY 2011
VL 47
IS 2
BP 6
EP +
PG 9
WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 731MS
UT WOS:000288111700003
ER
PT J
AU Cano, RJ
Loos, AC
Jensen, BJ
Britton, SM
Tuncol, G
Long, K
AF Cano, R. J.
Loos, A. C.
Jensen, B. J.
Britton, S. M.
Tuncol, G.
Long, K.
TI Epoxy/Glass and Polyimide (LaRC (TM) PETI-8)/Carbon Fiber Metal
Laminates Made by the VARTM Process
SO SAMPE JOURNAL
LA English
DT Article
ID RESINS
AB Recent work at NASA Langley Research Center (LaRC) has concentrated on developing new polyimide resin systems for advanced aerospace applications that can be processed without the use of an autoclave. Polyimide composites are very attractive for applications that require a high strength to weight ratio and thermal stability. Vacuum assisted resin transfer molding (VARTM) has shown the potential to reduce the manufacturing cost of composite structures. Fiber metal laminates (FML) made via this process with aluminum, glass fabric, and epoxy resins have been previously fabricated at LaRC. In this work, the VARTM process has been refined for epoxy/glass FMLs and extended to the fabrication of FMLs with titanium/carbon fabric layers and a polyimide system developed at NASA, LARC (TM) PETI-8. Resin flow pathways were introduced into the titanium foils to aid the infiltration of the polyimide resin. Injection temperatures in the range of 250-280 degrees C were required to achieve the necessary VARTM viscosities (< 10 Poise). Laminate quality and initial mechanical properties will be presented.
C1 [Cano, R. J.; Jensen, B. J.; Britton, S. M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Loos, A. C.; Tuncol, G.; Long, K.] Michigan State Univ, E Lansing, MI 48824 USA.
RP Cano, RJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 18
TC 1
Z9 1
U1 4
U2 14
PU SAMPE PUBLISHERS
PI COVINA
PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA
SN 0091-1062
J9 SAMPE J
JI Sampe J.
PD MAR-APR
PY 2011
VL 47
IS 2
BP 50
EP 58
PG 9
WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 731MS
UT WOS:000288111700005
ER
PT J
AU Numata, K
Chen, JR
Wu, ST
Abshire, JB
Krainak, MA
AF Numata, Kenji
Chen, Jeffrey R.
Wu, Stewart T.
Abshire, James B.
Krainak, Michael A.
TI Frequency stabilization of distributed-feedback laser diodes at 1572 nm
for lidar measurements of atmospheric carbon dioxide
SO APPLIED OPTICS
LA English
DT Article
ID DIFFERENTIAL ABSORPTION LIDAR; WAVELENGTH CALIBRATION LINES; PHOTONIC
CRYSTAL FIBERS; MODULATION SPECTROSCOPY; AMPLITUDE-MODULATION; PHASE
MODULATION; HIGH-POWER; DFB LASER; CORE; CO2
AB We demonstrate a wavelength-locked laser source that rapidly steps through six wavelengths distributed across a 1572.335 nm carbon dioxide (CO2) absorption line to allow precise measurements of atmospheric CO2 absorption. A distributed-feedback laser diode (DFB-LD) was frequency-locked to the CO2 line center by using a frequency modulation technique, limiting its peak-to-peak frequency drift to 0.3 MHz at 0.8 s averaging time over 72 hours. Four online DFB-LDs were then offset locked to this laser using phase-locked loops, retaining virtually the same absolute frequency stability. These online and two offline DFB-LDs were subsequently amplitude switched and combined. This produced a precise wavelength-stepped laser pulse train, to be amplified for CO2 measurements. (C) 2011 Optical Society of America
C1 [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Numata, Kenji; Chen, Jeffrey R.; Wu, Stewart T.; Abshire, James B.; Krainak, Michael A.] 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 Abshire, James/I-2800-2013
FU NASA
FX The authors gratefully acknowledge A. Stummer at the University of
Toronto for sharing technical details of his laser offset locking system
through website postings. They are also indebted to Y. Yin at YY labs,
Inc. for developing the custom MZM bias controllers, B. Merritt and the
modulator design team at JDSU Corp. for helpful discussions on the RAM
in the phase modulators, and J. Mao at NASA Goddard for providing
atmospheric CO2 absorption modeling results. R. DiSilvestre
at NASA Goddard machine shop and F. Kimpel at Fibertek, Inc. contributed
to the construction of the laser seeder system, and the authors are
appreciative of their skillful assistance. This work was supported by
the NASA Earth Science Technology Office Instrument Incubator Program
and the NASA Goddard Internal Research and Development program.
NR 44
TC 42
Z9 45
U1 1
U2 23
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 MAR 1
PY 2011
VL 50
IS 7
BP 1047
EP 1056
DI 10.1364/AO.50.001047
PG 10
WC Optics
SC Optics
GA 728CN
UT WOS:000287851800025
PM 21364729
ER
PT J
AU Abbasi, R
Abdou, Y
Abu-Zayyad, T
Adams, J
Aguilar, JA
Ahlers, M
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Bay, R
Alba, JLB
Beattie, K
Beatty, JJ
Bechet, S
Becker, JK
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Braun, J
Buitink, S
Carson, M
Chirkin, D
Christy, B
Clem, J
Clevermann, F
Cohen, S
Colnard, C
Cowen, DF
D'Agostino, MV
Danninger, M
Davis, JC
De Clercq, C
Demirors, L
Depaepe, O
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dierckxsens, M
Dreyer, J
Dumm, JP
Duvoort, MR
Ehrlich, R
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feusels, T
Filimonov, K
Finley, C
Foerster, MM
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Geisler, M
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Grant, D
Griesel, T
Gross, A
Grullon, S
Gurtner, M
Ha, C
Hallgren, A
Halzen, F
Han, K
Hanson, K
Helbing, K
Herquet, P
Hickford, S
Hill, GC
Hoffman, KD
Homeier, A
Hoshina, K
Hubert, D
Huelsnitz, W
Hulss, JP
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kemming, N
Kenny, P
Kiryluk, J
Kislat, F
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Koskinen, DJ
Kowalski, M
Kowarik, T
Krasberg, M
Krings, T
Kroll, G
Kuehn, K
Kuwabara, T
Labare, M
Lafebre, S
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lehmann, R
Lunemann, J
Madsen, J
Majumdar, P
Marotta, A
Maruyama, R
Mase, K
Matis, HS
Matusik, M
Meagher, K
Merck, M
Meszaros, P
Meures, T
Middell, E
Milke, N
Miller, J
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Nam, JW
Naumann, U
Niessen, P
Nygren, DR
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Ono, M
Panknin, S
Paul, L
de los Heros, CP
Petrovic, J
Piegsa, A
Pieloth, D
Porrata, R
Posselt, J
Price, PB
Prikockis, M
Przybylski, GT
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Rodrigues, JP
Roth, P
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Schlenstedt, S
Schmidt, T
Schukraft, A
Schultes, A
Schulz, O
Schunck, M
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Singh, K
Slipak, A
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stephens, G
Stezelberger, T
Stokstad, RG
Stoyanov, S
Strahler, EA
Straszheim, T
Sullivan, GW
Swillens, Q
Taavola, H
Taboada, I
Tamburro, A
Tarasova, O
Tepe, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Tosi, D
Turcan, D
van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
van Santen, J
Voge, M
Voigt, B
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Wikstrom, G
Williams, DR
Wischnewski, R
Wissing, H
Wolf, M
Woschnagg, K
Xu, C
Xu, XW
Yodh, G
Yoshida, S
Zarzhitsky, P
AF Abbasi, R.
Abdou, Y.
Abu-Zayyad, T.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Bay, R.
Alba, J. L. Bazo
Beattie, K.
Beatty, J. J.
Bechet, S.
Becker, J. K.
Becker, K. -H.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Buitink, S.
Carson, M.
Chirkin, D.
Christy, B.
Clem, J.
Clevermann, F.
Cohen, S.
Colnard, C.
Cowen, D. F.
D'Agostino, M. V.
Danninger, M.
Davis, J. C.
De Clercq, C.
Demiroers, L.
Depaepe, O.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dierckxsens, M.
Dreyer, J.
Dumm, J. P.
Duvoort, M. R.
Ehrlich, R.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feusels, T.
Filimonov, K.
Finley, C.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Geisler, M.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Grant, D.
Griesel, T.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Helbing, K.
Herquet, P.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Homeier, A.
Hoshina, K.
Hubert, D.
Huelsnitz, W.
Huelss, J. -P.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Joseph, J. M.
Kampert, K. H.
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
Kemming, N.
Kenny, P.
Kiryluk, J.
Kislat, F.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Koskinen, D. J.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Krings, T.
Kroll, G.
Kuehn, K.
Kuwabara, T.
Labare, M.
Lafebre, S.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Lehmann, R.
Luenemann, J.
Madsen, J.
Majumdar, P.
Marotta, A.
Maruyama, R.
Mase, K.
Matis, H. S.
Matusik, M.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Middell, E.
Milke, N.
Miller, J.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Nam, J. W.
Naumann, U.
Niessen, P.
Nygren, D. R.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Ono, M.
Panknin, S.
Paul, L.
de los Heros, C. Perez
Petrovic, J.
Piegsa, A.
Pieloth, D.
Porrata, R.
Posselt, J.
Price, P. B.
Prikockis, M.
Przybylski, G. T.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Rodrigues, J. P.
Roth, P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Schlenstedt, S.
Schmidt, T.
Schukraft, A.
Schultes, A.
Schulz, O.
Schunck, M.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Singh, K.
Slipak, A.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stephens, G.
Stezelberger, T.
Stokstad, R. G.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Sullivan, G. W.
Swillens, Q.
Taavola, H.
Taboada, I.
Tamburro, A.
Tarasova, O.
Tepe, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Tosi, D.
Turcan, D.
van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
van Santen, J.
Voge, M.
Voigt, B.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Wikstroem, G.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Wolf, M.
Woschnagg, K.
Xu, C.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
CA IceCube Collaboration
TI Constraints on high-energy neutrino emission from SN 2008D
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE supernovae: individual: SN 2008D; neutrinos; astroparticle physics
ID GAMMA-RAY BURST; ICECUBE DETECTOR; TRANSIENT 080109; MUON NEUTRINOS;
SUPERNOVA; TELESCOPE; MODEL; JET
AB SN 2008D, a core collapse supernova at a distance of 27 Mpc, was serendipitously discovered by the Swift satellite through an associated X-ray flash. Core collapse supernovae have been observed in association with long gamma-ray bursts and X-ray flashes and a physical connection is widely assumed. This connection could imply that some core collapse supernovae possess mildly relativistic jets in which high-energy neutrinos are produced through proton-proton collisions. The predicted neutrino spectra would be detectable by Cherenkov neutrino detectors like IceCube. A search for a neutrino signal in temporal and spatial correlation with the observed X-ray flash of SN 2008D was conducted using data taken in 2007-2008 with 22 strings of the IceCube detector. Events were selected based on a boosted decision tree classifier trained with simulated signal and experimental background data. The classifier was optimized to the position and a "soft jet" neutrino spectrum assumed for SN 2008D. Using three search windows placed around the X-ray peak, emission time scales from 100-10 000 s were probed. No events passing the cuts were observed in agreement with the signal expectation of 0.13 events. Upper limits on the muon neutrino flux from core collapse supernovae were derived for different emission time scales and the principal model parameters were constrained. While no meaningful limits can be given in the case of an isotropic neutrino emission, the parameter space for a jetted emission can be constrained. Future analyses with the full 86 string IceCube detector could detect up to similar to 100 events for a core-collapse supernova at 10 Mpc according to the soft jet model.
C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Braun, J.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Kappes, A.; Karle, A.; Kelley, J. L.; Krasberg, M.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subat & Radiat Phys, B-9000 Ghent, Belgium.
[Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Adams, J.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Auffenberg, J.; Becker, K. -H.; Gurtner, M.; Helbing, K.; Kampert, K. H.; Karg, T.; Matusik, M.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Barwick, S. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schlenstedt, S.; Spiering, C.; Tarasova, O.; Tosi, D.; Voigt, B.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
[Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium.
[Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Huelss, J. -P.; Krings, T.; Laihem, K.; Meures, T.; Nam, J. W.; Paul, L.; Schukraft, A.; Schunck, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wikstroem, G.] Stockholm Univ, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wikstroem, G.] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden.
[Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Singh, K.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Duvoort, M. R.] Univ Utrecht, SRON, Dept Phys & Astron, NL-3584 CC Utrecht, Netherlands.
[Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Kemming, N.; Kolanoski, H.; Lehmann, R.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Montaruli, T.] Univ Bari, I-70126 Bari, Italy.
[Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Kappes, A.] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany.
RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
EM mail@nickkemming.com
RI Taavola, Henric/B-4497-2011; Tamburro, Alessio/A-5703-2013; Hallgren,
Allan/A-8963-2013; Botner, Olga/A-9110-2013; Tjus, Julia/G-8145-2012;
Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar
Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar,
Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch,
Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012
OI Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft,
Anne/0000-0002-9112-5479; Perez de los Heros,
Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810;
Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819;
Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed
Lotfi/0000-0003-4410-5886; Auffenberg, Jan/0000-0002-1185-9094;
Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
Actis, Oxana/0000-0001-8851-3983; Wiebusch,
Christopher/0000-0002-6418-3008;
FU US National Science Foundation-Office of Polar Program; US National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; US Department of Energy; National Energy Research
Scientific Computing Center; Louisiana Optical Network Initiative
(LONI); Swedish Research Council; Swedish Polar Research Secretariat;
Knut and AliceWallenberg Foundation, Sweden; German Ministry for
Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG),
Germany; Fund for Scientific Research (FNRSFWO); Flanders Institute to
encourage scientific and technological research in industry (IWT);
Belgian Federal Science Policy Office (Belspo); the Netherlands
Organisation for Scientific Research (NWO)
FX We acknowledge the support from the following agencies: US National
Science Foundation-Office of Polar Program, US National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, US Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; Swedish Research Council, Swedish Polar
Research Secretariat, and Knut and AliceWallenberg Foundation, Sweden;
German Ministry for Education and Research (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Germany; Fund for Scientific Research
(FNRSFWO), Flanders Institute to encourage scientific and technological
research in industry (IWT), Belgian Federal Science Policy Office
(Belspo); the Netherlands Organisation for Scientific Research (NWO); M.
Ribordy acknowledges the support of the SNF (Switzerland); A. Kappes and
A. Gro acknowledge support by the EU Marie Curie OIF Program; J. P.
Rodrigues acknowledge support by the Capes Foundation, Ministry of
Education of Brazil.
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2011
VL 527
AR A28
DI 10.1051/0004-6361/201015770
PG 8
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SC Astronomy & Astrophysics
GA 723CP
UT WOS:000287484100043
ER
PT J
AU Gonzalez-Martin, O
Papadakis, I
Braito, V
Masegosa, J
Marquez, I
Mateos, S
Acosta-Pulido, JA
Martinez, MA
Ebrero, J
Esquej, P
O'Brien, P
Tueller, J
Warwick, RS
Watson, MG
AF Gonzalez-Martin, O.
Papadakis, I.
Braito, V.
Masegosa, J.
Marquez, I.
Mateos, S.
Acosta-Pulido, J. A.
Martinez, M. A.
Ebrero, J.
Esquej, P.
O'Brien, P.
Tueller, J.
Warwick, R. S.
Watson, M. G.
TI Suzaku observation of the LINER NGC4102
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: Seyfert; galaxies:
individual: NGC 4102; X-ray: galaxies
ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; SEYFERT 2 GALAXIES;
BLACK-HOLE MASS; X-RAY; NEARBY GALAXIES; EMISSION-LINE; XMM-NEWTON; HOST
GALAXIES; H-I
AB Context. Low-ionisation, nuclear emission-line region (LINER) nuclei are said to be different from other active galactic nuclei (AGN) due to the presence of complex absorbing structures along the line-of-sight and/or an inefficient mode of accretion onto the supermassive black hole. However, this is still open.
Aims. We investigate the broad band X-ray spectrum of NGC4102, one of the most luminous LINERs in the Swift/BAT survey.
Methods. We studied a 80 ks Suzaku spectrum of NGC4102, together with archival Chandra and Swift/BAT observations. We also studied the optical (3.5 m/TWIN at Calar Alto observatory) and near-infrared (WHT/LIRIS at Observatorio Roque los Muchachos) spectra that were taken at the same time as the Suzaku data.
Results. There is strong evidence that NGC4102 is a Compton-thick AGN, as suggested by the Swift/BAT detected intrinsic continuum and the presence of a strong narrow, neutral FeK alpha emission line. We have also detected ionised Fe-XXV emission lines in the Suzaku spectrum of the source. NGC4102 shows a variable soft excess found at a significantly higher flux state at the time of Suzaku observations when compared to Chandra observations. Finally, a complex structure of absorbers is seen with at least two absorbers besides the Compton-thick one, derived from the X-ray spectral analysis and the optical extinction.
Conclusions. All the signatures described in this paper strongly suggest that NGC4102 is a Compton-thick Type-2 AGN from the X-ray point of view. The "soft excess", the electron scattered continuum component, and the ionised iron emission line might arise from Compton-thin material photoionised by the AGN. From variability and geometrical arguments, this material should be located somewhere between 0.4 and 2 pc away from the nuclear source, inside the torus and perpendicular to the disc. The bolometric luminosity (L-bol = 1.4 x 10(43) erg s(-1)) and accretion rate ((m) over dot(Edd) = 5.4 x 10(-3)) are consistent with other low-luminosity AGN. However, the optical and near infrared spectra correspond to that of a LINER source. We suggest that the LINER classification might be due a different spectral energy distribution according to its steeper spectral index.
C1 [Gonzalez-Martin, O.; Papadakis, I.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece.
[Gonzalez-Martin, O.; Papadakis, I.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
Univ Leicester, Dept Phys & Astron, Leicester, Leics, England.
[Braito, V.; Mateos, S.; Esquej, P.; O'Brien, P.; Warwick, R. S.; Watson, M. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Masegosa, J.; Marquez, I.; Martinez, M. A.] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Acosta-Pulido, J. A.] Inst Astrofis Canarias, Tenerife 38205, La Laguna, Spain.
[Acosta-Pulido, J. A.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
[Martinez, M. A.] Univ Zaragoza, Inst Univ Matemat & Aplicac, Zaragoza 50009, Spain.
[Martinez, M. A.] Univ Zaragoza, Grp Mecan Espacial, Zaragoza 50009, Spain.
[Ebrero, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Tueller, J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Gonzalez-Martin, O (reprint author), Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece.
EM omaira@physics.uoc.gr
RI Papadakis, Iossif/C-3235-2011; Tueller, Jack/D-5334-2012; Marquez,
Isabel/A-1248-2009; XRAY, SUZAKU/A-1808-2009; Mateos,
Silvia/F-9524-2016;
OI Mateos, Silvia/0000-0002-1375-2389; Masegosa, J./0000-0002-3170-4137;
Marquez Perez, Isabel/0000-0003-2629-1945; Braito,
Valentina/0000-0002-2629-4989
FU EU [FP7-REGPOT 206469, ToK 39965]; Spanish grant [AYA2007-62190]; Junta
de Andalucia [TIC-114]; Excellence Project [P08-TIC-03531]; Spanish
research project [AYA2008-05572]; NWO, Netherlands Organization for
Scientific Research; STFC
FX We thank to the referee for his/her useful comments. This research made
use of data obtained from the Suzaku satellite, a collaborative mission
between the space agencies of Japan (JAXA) and the USA (NASA). This
research made use of data obtained from the Chandra Data Archive, and
software provided by the Chandra X-ray Center (CXC) in the application
package CIAO. Based on observations collected at the Centro Astronomico
Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck
Institut fur Astronomie and the Instituto de Astrofisica de Andalucia
(CSIC). This article is based on observations made with the William
Herschel Telescope operated in La Palma by the Isaac Newton Group in the
Spanish Observatory El Roque de los Muchachos. O. G. M. thanks M.
Guainazzi for useful discussion of this source. O. G. M. acknowledges
support by the EU FP7-REGPOT 206469 and ToK 39965 grants. I. M. and J.M.
acknowledge finalcial support from the Spanish grant AYA2007-62190 and
Junta de Andalucia TIC-114 and the Excellence Project P08-TIC-03531. M.
A. M. acknowledges the support by the Spanish research project
AYA2008-05572. The Space Research Organization of The Netherlands is
supported financially by NWO, the Netherlands Organization for
Scientific Research. PE acknowledges financial support from STFC.
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2011
VL 527
AR A142
DI 10.1051/0004-6361/201016097
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 723CP
UT WOS:000287484100157
ER
PT J
AU Shore, SN
Wahlgren, GM
Augusteijn, T
Liimets, T
Page, KL
Osborne, JP
Beardmore, AP
Koubsky, P
Slechta, M
Votruba, V
AF Shore, S. N.
Wahlgren, G. M.
Augusteijn, T.
Liimets, T.
Page, K. L.
Osborne, J. P.
Beardmore, A. P.
Koubsky, P.
Slechta, M.
Votruba, V.
TI The spectroscopic evolution of the symbiotic-like recurrent nova V407
Cygni during its 2010 outburst
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE novae, cataclysmic variables; stars: individual: V407 Cyg; stars:
individual: RS Oph; binaries: symbiotic; galaxies: active
ID DIFFUSE INTERSTELLAR BANDS; RS-OPHIUCHI; IA SUPERNOVAE; RAY-EMISSION;
BLAST WAVE; STARS; ULTRAVIOLET; SIMULATIONS; ABSORPTION; PHOTOMETRY
AB Context. V407 Cyg was, before 2010 Mar., known only as a D-type symbiotic binary system in which the Mira variable has a pulsation period of approximately 750 days, one of the longest known. On 2010 Mar. 10, it was discovered in outburst, eventually reaching V < 8. This is the first recorded nova event for this system, but it closely resembles the spectroscopic development of RS Oph, the prototypical symbiotic-like recurrent nova. It was also detected by Fermi above 100 MeV and displayed strong, likely nonthermal centimeter wavelength radio emission.
Aims. Unlike classical novae occurring in compact cataclysmic binary systems, for which the ejecta undergo free ballistic expansion, this explosion occurred within the dense, complex wind of a Mira variable companion. This paper concentrates on the development of the shock and its passage through the Mira wind. We also present some constraints on the binary system properties.
Methods. Using medium and high resolution ground-based optical spectra, visual and Swift UV photometry, and Swift X-ray spectrophotometry, we describe the behavior of the high-velocity profile evolution for this nova during its first three months.
Results. Using the diffuse interstellar bands visible in the high-resolution optical spectra, we obtain an extinction E(B - V) approximate to 0.45 +/- 0.05. The spectral type of the red giant during this period, when the star was at R minimum, was no earlier than M7 III. The peak of the X-ray emission occurred at about day 40 with a broad maximum and decline after day 50. The main changes in the optical spectrum began at around that time. The He II 4686 angstrom line first appeared between days 7 and 14 and initially displayed a broad, symmetric profile that is characteristic of all species before day 60. The profile development thereafter depended on ionization state. Low-excitation lines remained comparatively narrow, with v(rad,max) of order 200-400 km s(-1). They were systematically more symmetric than lines such as [Ca V], [Fe VII], [Fe X], and He II, all of which showed a sequence of profile changes going from symmetric to a blue wing similar to that of the low ionization species but with a red wing extended to as high as 600 km s(-1). The [O I] 6300, 6364 doublet showed a narrow wind-emission component near the rest velocity of the system and a broad component, 200-300 km s(-1), whose relative intensity increased in time. Forbidden lines of N II and O III had two separate contributors to the profiles, a broad line that increased in strength and velocity width, exceeding 200 km s(-1), and narrow components from a surrounding ionized region at higher velocity than the Mira wind. The Na I D doublet developed a broad component with similar velocity width to the other low-ionization species. The O VI Raman features observed in recent outbursts of RS Oph were not detected. We interpret these variations as aspherical expansion of the ejecta within the Mira wind. The blue side is from the shock penetrating into the wind while the red wing is from the low-density periphery. The maximum radial velocities obey power laws, v(max) similar to t(-n) with n approximate to 1/3 for red wing and approximate to 0.8 for the blue.
C1 [Shore, S. N.] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy.
[Shore, S. N.] Ist Nazl Fis Nucl, Sez Pisa, Pisa, Italy.
[Wahlgren, G. M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wahlgren, G. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Augusteijn, T.; Liimets, T.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Santa Cruz Tene, Spain.
[Liimets, T.] Tartu Observ, EE-61602 Toravere, Estonia.
[Page, K. L.; Osborne, J. P.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Koubsky, P.; Slechta, M.; Votruba, V.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic.
RP Shore, SN (reprint author), Univ Pisa, Dipartimento Fis Enrico Fermi, Largo B Pontecorvo 3, I-56127 Pisa, Italy.
EM shore@df.unipi.it; glenn.m.wahlgren@nasa.gov; tau@not.iac.es;
tiina@not.iac.es; kpa@star.le.ac.uk; julo@star.le.ac.uk;
apb@star.le.ac.uk; koubsky@sunstel.asu.cas.cz
RI Votruba, Viktor/G-9058-2014; Koubsky, Pavel/G-9031-2014; Slechta,
Miroslav/G-9048-2014
FU ESA PECS [98058]; NASA [NNG06GJ29G]; STFC; PhD School "Galileo Galilei",
Univ. of Pisa
FX P.K. was supported by ESA PECS grant No 98058. GMW acknowledges support
from NASA grant NNG06GJ29G. A.P.B., J.P.O. & K.L.P. acknowledge the
support of STFC. We thank C.-C. Cheung, J. Jose, K. Mukai, U. Munari,
Quillo, and C. Rossi for discussions. We also thank the (anonymous)
referee for helpful suggestions. S.N.S. acknowledges support from the
PhD School "Galileo Galilei", Univ. of Pisa. Special thanks J.
Mikolajewska for valuable discussions of this and related systems during
her visit to Pisa in May 2010, and the Fermi LAT group (INFN-Pisa) for
collaboration. Some spectra at Ondrejov were taken by L. Kotkova, P.
Skoda, and J. Polster. We have made extensive use of the Astrophysics
Data System (ADS), SIMBAD (CDS), and the MAST archive (STScI) in the
course of this work.
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2011
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SC Astronomy & Astrophysics
GA 723CP
UT WOS:000287484100113
ER
PT J
AU Staubert, R
Pottschmidt, K
Doroshenko, V
Wilms, J
Suchy, S
Rothschild, R
Santangelo, A
AF Staubert, R.
Pottschmidt, K.
Doroshenko, V.
Wilms, J.
Suchy, S.
Rothschild, R.
Santangelo, A.
TI Finding a 24-day orbital period for the X-ray binary 1A 1118-616
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE binaries: general; stars: neutron; X-rays: general; X-rays: binaries;
X-rays: individuals: 1A 1118-616; ephemerides
ID SAX J2103.5+4545; DISCOVERY; OUTBURST; X-3
AB We report the first determination of the binary period and orbital ephemeris of the Be X-ray binary containing the pulsar 1A 1118-616 (35 years after the discovery of the source). The orbital period is found to be P(orb) = 24.0 +/- 0.4 days. The source was observed by RXTE during its last large X-ray outburst in January 2009, which peaked at MJD 54845.4, by taking short observations every few days, covering an elapsed time comparable to the orbital period. Using the phase connection technique, pulse arrival time delays could be measured and an orbital solution determined. The data are consistent with a circular orbit and the time of 90 degrees longitude was found to be T(pi/2) = MJD 54845.37(10), which is coincident with that of the peak X-ray flux.
C1 [Staubert, R.; Doroshenko, V.; Santangelo, A.] Univ Tubingen IAAT, Abt Astron, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol CRESST, Baltimore, MD 21250 USA.
[Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
[Suchy, S.; Rothschild, R.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
RP Staubert, R (reprint author), Univ Tubingen IAAT, Abt Astron, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM staubert@astro.uni-tuebingen.de
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Doroshenko, Victor/0000-0001-8162-1105
FU DLR [50 OR 0702]; NASA [NAS5-30720]
FX We acknowledge the support through DLR grant 50 OR 0702. R.St. likes to
thank Klaus Werner and Dima Klochkov for discussions about the optical
companion and the analysis of the ASM light curve, respectively. R. E.
R. and S. S. acknowledge the support under NASA contract NAS5-30720. We
thank Robin Corbet for pointing us to SAX J2103.5+4545 and for his data
collection of the Corbet-diagram.
NR 25
TC 9
Z9 9
U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2011
VL 527
AR A7
DI 10.1051/0004-6361/201015737
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 723CP
UT WOS:000287484100022
ER
PT J
AU Sturm, R
Haberl, F
Coe, MJ
Bartlett, ES
Buckley, DAH
Corbet, RHD
Ehle, M
Filipovic, MD
Hatzidimitriou, D
Mereghetti, S
La Palombara, N
Pietsch, W
Tiengo, A
Townsend, LJ
Udalski, A
AF Sturm, R.
Haberl, F.
Coe, M. J.
Bartlett, E. S.
Buckley, D. A. H.
Corbet, R. H. D.
Ehle, M.
Filipovic, M. D.
Hatzidimitriou, D.
Mereghetti, S.
La Palombara, N.
Pietsch, W.
Tiengo, A.
Townsend, L. J.
Udalski, A.
TI The XMM-Newton survey of the Small Magellanic Cloud: discovery of the
11.866 s Be/X-ray binary pulsar XMMU J004814.0-732204 (SXP11.87)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: individual: Small Magellanic Cloud; galaxies: stellar content;
stars: emission-line, Be; stars: neutron; X-rays: binaries
ID STAR; CATALOG; LONG; OUTBURST; BEHAVIOR
AB Aims. One of the goals of the XMM-Newton survey of the Small Magellanic Cloud is to study the Be/X-ray binary population. During one of our first survey observations, a bright new transient -XMMU 004814.0-732204 -was discovered.
Methods. We present the analysis of the EPIC X-ray data, together with optical observations, to investigate the spectral and temporal characteristics of XMMU J004814.0-732204.
Results. We found coherent X-ray pulsations in the EPIC data with a period of (11.86642 +/- 0.00017) s. The X-ray spectrum can be modelled by an absorbed power law with an indication for a soft excess. Depending on the modelling of the soft X-ray spectrum, the photon index ranges between 0.53 and 0.66. We identify the optical counterpart as a B = 14.9 mag star that was monitored during the MACHO and OGLE-III projects. The optical light curves show regular outbursts by similar to 0.5 mag in B and R and up to 0.9 mag in I, which repeat on a time scale of about 1000 days. The OGLE-III optical colours of the star are consistent with an early B spectral type. An optical spectrum obtained at the 1.9m telescope of the South African Astronomical Observatory in December 2009 shows Ha emission with an equivalent width of 3.5 +/- 0.6 angstrom.
Conclusions. The X-ray spectrum and the detection of pulsations suggest that XMMU J004814.0-732204 is a new high-mass X-ray binary pulsar in the SMC. The long term variability and the Ha emission line in the spectrum of the optical counterpart identify it as a Be/X-ray binary system.
C1 [Sturm, R.; Haberl, F.; Pietsch, W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Coe, M. J.; Bartlett, E. S.; Townsend, L. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Buckley, D. A. H.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Corbet, R. H. D.] Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ehle, M.] ESA, XMM Newton Sci Operat Ctr, ESAC, Madrid 28691, Spain.
[Filipovic, M. D.] Univ Western Sydney, Penrith, NSW 1797, Australia.
[Hatzidimitriou, D.] Univ Athens, Dept Astrophys Astron & Mech, Athens 15784, Greece.
[Hatzidimitriou, D.] IESL, Fdn Res & Technol Hellas, Athens, Greece.
[Mereghetti, S.; La Palombara, N.; Tiengo, A.] Ist Astrofis Spaziale & Fis Cosm Milano, INAF, I-20133 Milan, Italy.
[Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Sturm, R (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM rsturm@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 Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur
Luft- und Raumfahrt (BMWI/DLR) [FKZ 50 OX 0001, FKZ 50 OR 0907];
Max-Planck Society; ASI [I/088/06/0]; University of Southampton;
MNiSW/BST
FX 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. R. S.
acknowledges support from the BMWI/DLR grant FKZ 50 OR 0907. S.M., N.L.,
and A.T. acknowledge the support of ASI through contract I/088/06/0.
L.J.T. is in receipt of a University of Southampton Mayflower
Scholarship. A. U. acknowledges support from the MNiSW/BST grant.
NR 41
TC 10
Z9 10
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2011
VL 527
AR A131
DI 10.1051/0004-6361/201015798
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 723CP
UT WOS:000287484100146
ER
PT J
AU Wang, S
Bergin, EA
Crockett, NR
Goldsmith, PF
Lis, DC
Pearson, JC
Schilke, P
Bell, TA
Comito, C
Blake, GA
Caux, E
Ceccarelli, C
Cernicharo, J
Daniel, F
Dubernet, ML
Emprechtinger, M
Encrenaz, P
Gerin, M
Giesen, TF
Goicoechea, JR
Gupta, H
Herbst, E
Joblin, C
Johnstone, D
Langer, WD
Latter, WB
Lord, SD
Maret, S
Martin, PG
Melnick, GJ
Menten, KM
Morris, P
Muller, HSP
Murphy, JA
Neufeld, DA
Ossenkopf, V
Perault, M
Phillips, TG
Plume, R
Qin, SL
Schlemmer, S
Stutzki, J
Trappe, N
van der Tak, FFS
Vastel, C
Yorke, HW
Yu, S
Zmuidzinas, J
AF Wang, S.
Bergin, E. A.
Crockett, N. R.
Goldsmith, P. F.
Lis, D. C.
Pearson, J. C.
Schilke, P.
Bell, T. A.
Comito, C.
Blake, G. A.
Caux, E.
Ceccarelli, C.
Cernicharo, J.
Daniel, F.
Dubernet, M-L
Emprechtinger, M.
Encrenaz, P.
Gerin, M.
Giesen, T. F.
Goicoechea, J. R.
Gupta, H.
Herbst, E.
Joblin, C.
Johnstone, D.
Langer, W. D.
Latter, W. B.
Lord, S. D.
Maret, S.
Martin, P. G.
Melnick, G. J.
Menten, K. M.
Morris, P.
Mueller, H. S. P.
Murphy, J. A.
Neufeld, D. A.
Ossenkopf, V.
Perault, M.
Phillips, T. G.
Plume, R.
Qin, S-L
Schlemmer, S.
Stutzki, J.
Trappe, N.
van der Tak, F. F. S.
Vastel, C.
Yorke, H. W.
Yu, S.
Zmuidzinas, J.
TI Herschel observations of EXtra-Ordinary Sources (HEXOS): Methanol as a
probe of physical conditions in Orion KL
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: abundances; ISM: molecules
ID MOLECULAR CLOUDS; STAR-FORMATION; SUBMILLIMETER; LINE; MILLIMETER;
EMISSION; DATABASE; REGION; HIFI; TOOL
AB We have examined methanol emission from Orion KL with the Herschel/HIFI instrument, and detected two methanol bands centered at 524 GHz and 1061 GHz. The 524 GHz methanol band (observed in HIFI band 1a) is dominated by the isolated Delta J = 0, K = -4 -> -3, v(t) = 0 Q branch, and includes 25 E-type and 2 A-type transitions. The 1061 GHz methanol band (observed in HIFI band 4b) is dominated by the Delta J = 0, K = 7 -> 6, v(t) = 0 Q branch transitions which are mostly blended. We have used the isolated E-type vt = 0 methanol transitions to explore the physical conditions in the molecular gas. With HIFI's high velocity resolution, the methanol emission contributed by different spatial components along the line of sight toward Orion KL (hot core, low velocity flow, and compact ridge) can be distinguished and studied separately. The isolated transitions detected in these bands cover a broad energy range (upper state energy ranging from 80 K to 900 K), which provides a unique probe of the thermal structure in each spatial component. The observations further show that the compact ridge is externally heated. These observations demonstrate the power of methanol lines as probes of the physical conditions in warm regions in close proximity to young stars.
C1 [Wang, S.; Bergin, E. A.; Crockett, N. R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Goldsmith, P. F.; Pearson, J. C.; Gupta, H.; Langer, W. D.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lis, D. C.; Bell, T. A.; Emprechtinger, M.; Phillips, T. G.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA.
[Schilke, P.; Comito, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Schilke, P.; Giesen, T. F.; Mueller, H. S. P.; Qin, S-L; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France.
[Caux, E.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France.
[Ceccarelli, C.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France.
[Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain.
[Daniel, F.; Perault, M.] Observ Paris, CNRS, UMR8112, LERMA, F-75231 Paris 05, France.
[Daniel, F.] Ecole Normale Super, F-75231 Paris 05, France.
[Dubernet, M-L] Univ Paris 06, UMR7092, LPMAA, Paris, France.
[Dubernet, M-L; Ossenkopf, V.] Observ Paris, UMR8102, LUTH, Meudon, France.
[Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Herbst, E.] Ohio State Univ, Dept Astron & Chem, Columbus, OH 43210 USA.
[Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Latter, W. B.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Murphy, J. A.; Trappe, N.] Natl Univ Ireland, Maynooth, Kildare, Ireland.
[Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ossenkopf, V.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
RP Wang, S (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM shiya@umich.edu
RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe,
Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016;
OI Giesen, Thomas /0000-0002-2401-0049; Schlemmer,
Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; Maret,
Sebastien/0000-0003-1104-4554; Mueller, Holger/0000-0002-0183-8927
FU NASA
FX HIFI has been designed and built by a consortium of institutes and
university departments from across Europe, Canada and the United States
under the leadership of SRON Netherlands Institute for Space Research,
Groningen, The Netherlands and with major contributions from Germany,
France and the 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; The Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain:
Observatorio Astronmico Nacional (IGN), Centro de Astrobiologa
(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. The HEXOS team also is grateful to the HIFI
instrument team for building a fantastic instrument. Support for this
work was provided by NASA through an award issued by JPL/Caltech.
NR 23
TC 24
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U1 0
U2 11
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2011
VL 527
AR A95
DI 10.1051/0004-6361/201015079
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 723CP
UT WOS:000287484100110
ER
PT J
AU Pavelsky, TM
Boe, J
Hall, A
Fetzer, EJ
AF Pavelsky, Tamlin M.
Boe, Julien
Hall, Alex
Fetzer, Eric J.
TI Atmospheric inversion strength over polar oceans in winter regulated by
sea ice
SO CLIMATE DYNAMICS
LA English
DT Article
DE Temperature inversion; Sea ice; Arctic; Antarctic; AIRS
ID TEMPERATURE INVERSIONS; ANTARCTIC TEMPERATURE; SURFACE-TEMPERATURE;
ERA-40 REANALYSIS; CLEAR-SKY; NCEP-NCAR; OSCILLATION; REGIONS; OZONE;
MODEL
AB Low-level temperature inversions are a common feature of the wintertime troposphere in the Arctic and Antarctic. Inversion strength plays an important role in regulating atmospheric processes including air pollution, ozone destruction, cloud formation, and negative longwave feedback mechanisms that shape polar climate response to anthropogenic forcing. The Atmospheric Infrared Sounder (AIRS) instrument provides reliable measures of spatial patterns in mean wintertime inversion strength when compared with available radiosonde observations and reanalysis products. Here, we examine the influence of sea ice concentration on inversion strength in the Arctic and Antarctic. Correlation of inversion strength with mean annual sea ice concentration, likely a surrogate for the effective thermal conductivity of the wintertime ice pack, yields strong, linear relationships in the Arctic (r = 0.88) and Antarctic (r = 0.86). We find a substantially greater (stronger) linear relationship between sea ice concentration and surface air temperature than with temperature at 850 hPa, lending credence to the idea that sea ice controls inversion strength through modulation of surface heat fluxes. As such, declines in sea ice in either hemisphere may imply weaker mean inversions in the future. Comparison of mean inversion strength in AIRS and global climate models (GCMs) suggests that many GCMs poorly characterize mean inversion strength at high latitudes.
C1 [Pavelsky, Tamlin M.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA.
[Boe, Julien; Hall, Alex] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Fetzer, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pavelsky, TM (reprint author), Univ N Carolina, Dept Geol Sci, CB 3315, Chapel Hill, NC 27599 USA.
EM pavelsky@unc.edu
RI Hall, Alex/D-8175-2014
FU National Science Foundation [ARC-0714083, ATM-0735056]
FX This research was funded by the National Science Foundation under grants
ARC-0714083 and ATM-0735056. Opinions, findings, or recommendations
expressed here are those of the authors and do not necessarily reflect
NSF views. We acknowledge the modeling groups, the Program for Climate
Model Diagnosis and Intercomparison (PCMDI) and the WCRP's Working Group
in Coupled Modeling (WGCM) for their roles in making available the WCRP
CMIP3 multi-model dataset. Support for this dataset is provided by the
Office of Science, U.S. Department of Energy. ECMWF ERA-40 data used in
this study have been obtained from the ECMWF data server.
NR 38
TC 30
Z9 31
U1 4
U2 21
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
J9 CLIM DYNAM
JI Clim. Dyn.
PD MAR
PY 2011
VL 36
IS 5-6
BP 945
EP 955
DI 10.1007/s00382-010-0756-8
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 729CB
UT WOS:000287924400008
ER
PT J
AU Wu, LL
Beard, BL
Roden, EE
Johnson, CM
AF Wu, Lingling
Beard, Brian L.
Roden, Eric E.
Johnson, Clark M.
TI Stable Iron Isotope Fractionation Between Aqueous Fe(II) and Hydrous
Ferric Oxide
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID MOSSBAUER-SPECTROSCOPY; FERRIHYDRITE; HEMATITE; SILICA; FE;
TRANSFORMATION; OXIDATION; GOETHITE; MINERALS; SURFACE
AB Despite the ubiquity of poorly crystalline ferric hydrous oxides (HFO, or ferrihydrite) in natural environments, stable Fe isotopic fractionation between HFO and other Fe phases remains unclear. In particular, it has been difficult: to determine equilibrium Fe isotope fractionation between aqueous Fe(II) and HFO due to fast transformation of the latter to more stable minerals. Here we used HFO stabilized by the presence of dissolved silica (2.14 mM), or a Si-HFO coprecipitate, to determine an equilibrium Fe(II) HFO fractionation factor using a three-isotope method. Iron isotope exchange between Fe(II) and HFO was rapid and near complete with the Si HFO coprecipitate, and rapid but incomplete for HFO in the resence of dissolved silica, the latter case likely reflecting blockage of oxide surface sites by sorbed silica. Equilibrium Fe(II)-HFO (56)Fe/(54)Fe fractionation factors of -3.17 +/- 0.08 (2 sigma)parts per thousand and -2.58 +/- 0.14 (2 sigma)parts per thousand were obtained for HFO plus silica and the Si-HFO coprecipitate, respectively. Structural similarity between ferrihydrite and hematite, as suggested by spectroscopic studies, combined with the minor isotopic effect of dissolved silica, imply that the true equilibrium Fe(II)-HFO (56)Fe/(54)Fe fractionation factor in the absence of silica may be similar to-3.2 parts per thousand. These results provide a critical interpretive context for inferring the stable isotope effects of Fe redox cycling in nature.
C1 [Wu, Lingling; Beard, Brian L.; Roden, Eric E.; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Wu, Lingling; Beard, Brian L.; Roden, Eric E.; Johnson, Clark M.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA.
RP Wu, LL (reprint author), Univ Wisconsin, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA.
EM lwu@geology.wisc.edu
RI Wu, Lingling/E-4087-2010
OI Wu, Lingling/0000-0002-8211-5754
FU NASA Astrobiology Institute
FX We thank Hiromi Konishi for TEM work. We also thank Michelle Scherer and
her group at University of Iowa for help with preparation of
57Fe-enriched aqueous ferrous iron. Two anonymous reviewer's
comments improved this manuscript. This research was supported by the
NASA Astrobiology Institute.
NR 42
TC 47
Z9 49
U1 3
U2 60
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD MAR 1
PY 2011
VL 45
IS 5
BP 1847
EP 1852
DI 10.1021/es103171x
PG 6
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 725HZ
UT WOS:000287637100017
PM 21294566
ER
PT J
AU Meneghini, R
Jones, JA
AF Meneghini, Robert
Jones, Jeffrey A.
TI Standard Deviation of Spatially Averaged Surface Cross Section Data From
the TRMM Precipitation Radar
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Atmospheric attenuation; normalized radar cross section (NRCS); surface
cross section; Tropical Rainfall Measuring Mission (TRMM) Precipitation
Radar (PR)
ID RAIN-RATE; ATTENUATION
AB We investigate the spatial variability of the normalized radar cross section of the surface (NRCS or sigma(0)) derived from measurements of the Tropical Rainfall Measuring Mission (TRMM) Precipitation Radar (PR) for the period from 1998 to 2009. The purpose of this letter is to understand the way in which the sample standard deviation (SSD) of the sigma(0) data changes as a function of spatial resolution, incidence angle, and surface type (land/ocean). The results have implications regarding the accuracy by which the path-integrated attenuation (PIA) from precipitation can be inferred by the use of surface-scattering properties.
C1 [Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jones, Jeffrey A.] Wyle Informat Syst Inc, Mclean, VA 22102 USA.
RP Meneghini, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Robert.Meneghini-1@nasa.gov; Jeffrey.A.Jones-3@nasa.gov
NR 8
TC 6
Z9 7
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD MAR
PY 2011
VL 8
IS 2
BP 293
EP 297
DI 10.1109/LGRS.2010.2064755
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 725PZ
UT WOS:000287659300022
ER
PT J
AU Cooper, M
Douglas, G
Perchonok, M
AF Cooper, Maya
Douglas, Grace
Perchonok, Michele
TI Developing the NASA Food System for Long-Duration Missions
SO JOURNAL OF FOOD SCIENCE
LA English
DT Review
DE food packaging; food safety; Mars; shelf life; space food
ID STORAGE-CONDITIONS; ASCORBIC-ACID; DEGRADATION; SPACE; KINETICS;
THIAMIN; FUTURE; RATES
AB Even though significant development has transformed the space food system over the last 5 decades to attain more appealing dietary fare for low-orbit space crews, the advances do not meet the need for crews that might travel to Mars and beyond. It is estimated that a food system for a long-duration mission must maintain organoleptic acceptability, nutritional efficacy, and safety for a 3- to 5-y period to be viable. In addition, the current mass and subsequent waste of the food system must decrease significantly to accord with the allowable volume and payload limits of the proposed future space vehicles. Failure to provide the appropriate food or to optimize resource utilization introduces the risk that an inadequate food system will hamper mission success and/or threaten crew performance. Investigators for the National Aeronautics and Space Administration (NASA) Advanced Food Technology (AFT) consider identified concerns and work to mitigate the risks to ensure that any new food system is adequate for the mission. Yet, even with carefully planned research, some technological gaps remain. NASA needs research advances to develop food that is nutrient-dense and long-lasting at ambient conditions, partial gravity cooking processes, methods to deliver prescribed nutrients over time, and food packaging that meets the mass, barrier, and processing requirements of NASA. This article provides a brief review of research in each area, details the past AFT research efforts, and describes the remaining gaps that present barriers to achieving a food system for long exploration missions.
C1 [Perchonok, Michele] NASA, Lyndon B Johnson Space Ctr, Habitabil & Human Factors Div, Houston, TX 77058 USA.
[Cooper, Maya] Lockheed Martin Informat Syst & Global Serv, Houston, TX 77058 USA.
[Douglas, Grace] N Carolina State Univ, Raleigh, NC 27695 USA.
RP Perchonok, M (reprint author), NASA, Lyndon B Johnson Space Ctr, Habitabil & Human Factors Div, Mail Code SF3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM michele.h.perchonok@nasa.gov
NR 39
TC 11
Z9 11
U1 4
U2 30
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-1147
J9 J FOOD SCI
JI J. Food Sci.
PD MAR
PY 2011
VL 76
IS 2
BP R40
EP R48
DI 10.1111/j.1750-3841.2010.01982.x
PG 9
WC Food Science & Technology
SC Food Science & Technology
GA 728EV
UT WOS:000287858000005
PM 21535783
ER
PT J
AU Tigelaar, DM
Palker, AE
He, RH
Scheiman, DA
Petek, T
Savinell, R
Yoonessi, M
AF Tigelaar, Dean M.
Palker, Allyson E.
He, Ronghuan
Scheiman, Daniel A.
Petek, Tyler
Savinell, Robert
Yoonessi, Mitra
TI Synthesis and properties of sulfonated and unsulfonated poly(arylene
ether triazine)s with pendant diphenylamine groups for fuel cell
applications
SO JOURNAL OF MEMBRANE SCIENCE
LA English
DT Article
DE Polymer electrolyte; Poly(arylene ether); Proton exchange membrane;
Phase separation
ID POLYMER ELECTROLYTE MEMBRANES; AROMATIC POLYETHERS; PYRIDINE UNITS;
PROTON; IONOMERS; COPOLYMERS; STABILITY; ACID; CONDUCTIVITY; SCATTERING
AB A series of poly(arylene ether triazine) homopolymers were synthesized that contain pendant diphenylamine groups. The polymers had inherent viscosities from 0.66 to 1.01 dL/g in DMAc at 25 degrees C, thermal stabilities > 500 degrees C in air, glass transition temperatures from 156 degrees C to 309 degrees C, and solubilities that depended upon the bis(4-fluorophenyl) monomer that was used for polymerization. Polymers could be sulfonated with chlorosulfonic acid exclusively at the para position of the diphenylamine rings, with ion exchange capacities from 1.88 to 2.12 meq/g. Transmission electron microscopy images show that the morphology of the sulfonated polymer films depends on the functional group in the polymer backbone. Polymers containing sulfone groups exhibited small ionic clusters within a uniform ion-containing background, while polymers with ketone and isophthaloyl groups exhibited phase separation with different sizes of spherical hydrophilic clusters. The uniform distribution of ionic groups within polymers that contain sulfone groups resulted in higher proton conductivity, 0.11 S/cm at 90 degrees C and 100% relative humidity, in spite of having a lower degree of sulfonation and water uptake. Small angle neutron scattering data also shows this film has a robust morphology that does not change as a function of temperature or by counterion exchange. Films cast from unsulfonated polymers that contained phosphine oxide groups in the polymer backbone, as well polymer blends with polybenzimidazole soaked in 85% phosphoric acid at 75 C, had phosphoric acid uptakes above 350 wt%, and as high as 830 wt%. However, these films lost dimensional stability at elevated temperatures. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Tigelaar, Dean M.; Palker, Allyson E.; Scheiman, Daniel A.; Yoonessi, Mitra] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[He, Ronghuan] Northeastern Univ, Dept Chem, Shenyang 110819, Peoples R China.
[Scheiman, Daniel A.] Arctic Slope Reg Corp, Barrow, AK USA.
[Petek, Tyler; Savinell, Robert] Case Western Reserve Univ, Dept Chem Engn, Cleveland, OH 44106 USA.
RP Tigelaar, DM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM dean.m.tigelaar@nasa.gov
RI He, Ronghuan/G-5702-2011
FU NASA NRA [NNC07BA13B]
FX Thank you to David Hull for performing TEM experiments. Thank you to
Derek Quade for performing tensile testing. Thank you to Hossein
Ghassemi at CWRU for helpful discussions. DMT was funded by NASA NRA
contract NNC07BA13B.
NR 40
TC 16
Z9 16
U1 2
U2 32
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0376-7388
J9 J MEMBRANE SCI
JI J. Membr. Sci.
PD MAR 1
PY 2011
VL 369
IS 1-2
BP 455
EP 465
DI 10.1016/j.memsci.2010.12.018
PG 11
WC Engineering, Chemical; Polymer Science
SC Engineering; Polymer Science
GA 727VY
UT WOS:000287832200053
ER
PT J
AU Lehnert, H
Stone, RP
AF Lehnert, Helmut
Stone, Robert P.
TI Craniella sputnika sp nov (Porifera: Spirophorida: Tetillidae) from the
Aleutian Islands, Alaska, with suggested nomenclatural changes for the
genera Tetilla and Craniella
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE Porifera; Spirophorida; Tetillidae; Craniella; Tetilla; taxonomy; new
species; Aleutian Islands
ID USA; DEMOSPONGIAE
AB A new species of Craniella from the Aleutian Islands is described. Craniella sputnika sp. nov. differ from all other species of Craniella in its habitus, absence of microscleres and size of spicules. The name refers to its resemblance to Earth's first artificial satellite, due to its spherical body with long spines. The new species was observed growing on another demosponge, Myxilla sp. We propose transferring two species currently in Craniella to Tetilla (Craniella ellipsoidea Hoshino, 1982 and Craniella laminaris (George & Wilson, 1919)) and two subspecies (Craniella globosa anamonaena Tanita, 1968 and Craniella laminaris symmetrica (Wilson, 1931)) from Craniella to Tetilla. As Craniella globosa anamonaena Tanita, 1968, is actually a species of Tetilla we suggest raising the subspecies to species rank as Tetilla anamonaena. Conversely we think that two species, Tetilla ovata (Thiele, 1898) and Tetilla hamatum Koltun, 1966 should be transferred to Craniella.
C1 [Stone, Robert P.] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, Juneau, AK 99801 USA.
RP Lehnert, H (reprint author), Eichenstr 14, D-86507 Oberottmarshausen, Germany.
EM Helm.Lehnert@t-online.de
FU NOAA/NMFS
FX Thanks to the crew of the RV 'Velero' and the submersible 'Delta' for
friendly and professional support during the field trip. Thanks also to
Wolfgang Heimler, Institute fur Entwicklungsbiologie, Erlangen
University and Wolfgang Christel, IPAT-Uni-Erlangen, Germany, who
operated the SEM. Thanks to three anonymous referees who helped to
improve the manuscript; special thanks to Tom Hourigan (NOAA) for his
continued support of deep-sea research in the North Pacific Ocean and
for making funds for this project available through the NOAA Deep Sea
Coral Research and Technology Program. H. L. was funded by a contract
from NOAA/NMFS.
NR 27
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U1 0
U2 0
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
EI 1469-7769
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD MAR
PY 2011
VL 91
IS 2
SI SI
BP 321
EP 328
DI 10.1017/S0025315410001025
PG 8
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 729HX
UT WOS:000287940400004
ER
PT J
AU Datsko, BY
Gafiychuk, VV
AF Datsko, B. Y.
Gafiychuk, V. V.
TI Chaotic dynamics in Bonhoffer-van der Pol fractional reaction-diffusion
system
SO SIGNAL PROCESSING
LA English
DT Article
DE Fractional differential equation; Anomalous diffusion;
Reaction-diffusion; Pattern formation; Pattern recognition; Chaotic
dynamics; Applications
ID PATTERN-FORMATION; ORDER CONTROLLERS; WAVES; TRANSPORT; NETWORKS;
EQUATION
AB In this article we analyze the linear stability of nonlinear fractional reaction-diffusion systems. As an example, the reaction-diffusion model with cubic nonlinearity is considered. By computer simulation, it was shown that in such simplest system, a complex nonlinear dynamics, which includes spatially non-homogeneous oscillations and spatio-temporal chaos, takes place. Possible applications of the fractional reaction-diffusion system for signal processing and pattern recognition systems are presented. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Datsko, B. Y.] Natl Acad Sci, Inst Appl Problems Mech & Math, UA-79063 Lvov, Ukraine.
[Gafiychuk, V. V.] SGT Inc, Greenbelt, MD 20770 USA.
[Gafiychuk, V. V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Datsko, BY (reprint author), Natl Acad Sci, Inst Appl Problems Mech & Math, Naukova 3B, UA-79063 Lvov, Ukraine.
EM b_datsko@yahoo.com; vagaf@yahoo.com
NR 55
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U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-1684
J9 SIGNAL PROCESS
JI Signal Process.
PD MAR
PY 2011
VL 91
IS 3
SI SI
BP 452
EP 460
DI 10.1016/j.sigpro.2010.04.004
PG 9
WC Engineering, Electrical & Electronic
SC Engineering
GA 730MZ
UT WOS:000288038800009
ER
PT J
AU Boersma, C
Bauschlicher, CW
Ricca, A
Mattioda, AL
Peeters, E
Tielens, AGGM
Allamandola, LJ
AF Boersma, C.
Bauschlicher, C. W., Jr.
Ricca, A.
Mattioda, A. L.
Peeters, E.
Tielens, A. G. G. M.
Allamandola, L. J.
TI POLYCYCLIC AROMATIC HYDROCARBON FAR-INFRARED SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: lines and bands; methods: laboratory; methods:
numerical; molecular data; techniques: spectroscopic
ID MU-M; PROTOPLANETARY NEBULAE; EMISSION FEATURES; ISO SPECTROSCOPY; PAHS;
SPECTRA; MOLECULE; ROTATION; DATABASE; COMPACT
AB The far-IR characteristics of astrophysically relevant polycyclic aromatic hydrocarbons ( PAHs) averaging in size around 100 carbon atoms have been studied using the theoretical spectra in the NASA Ames PAH IR Spectroscopic Database. These spectra were calculated using density functional theory. Selections of PAH species are made, grouped together by common characteristics or trends, such as size, shape, charge, and composition, and their far-IR spectra compared. The out-of-plane modes involving the entire molecule are explored in detail, astronomical relevance is assessed, and an observing strategy is discussed. It is shown that PAHs produce richer far-IR spectra with increasing size. PAHs also produce richer far-IR spectra with increasing number of irregularities. However, series of irregular-shaped PAHs with the same compact core have common "Jumping-Jack" modes that "pile up" at specific frequencies in their average spectrum. For the PAHs studied here, around 100 carbon atoms in size, this band falls near 50 mu m. PAH charge and nitrogen inclusion affect band intensities but have little effect on far-IR band positions. Detailed analysis of the two-dimensional, out-of-plane bending "drumhead" modes in the coronene and pyrene "families" and the one-dimensional, out-of-plane bending "bar" modes in the acene "family" show that these molecular vibrations can be treated as classical vibrating sheets and bars of graphene, respectively. The analysis also shows that the peak position of these modes is very sensitive to the area of the emitting PAH and does not depend on the particular geometry. Thus, these longest wavelength PAH bands could provide a unique handle on the size of the largest species in the interstellar PAH family. However, these bands are weak. Observing highly excited regions showing the mid-IR bands in which the emission from classical dust peaks at short wavelengths offers the best chance of detecting PAH emission in the far-IR. For these regions sensitivity is not an issue, spectral contrast is maximized and the PAH population is only comprised of highly stable, compact symmetric PAHs, such as the members of the pyrene and coronene "families" discussed in detail here.
C1 [Boersma, C.; Bauschlicher, C. W., Jr.; Ricca, A.; Mattioda, A. L.; Tielens, A. G. G. M.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ricca, A.; Peeters, E.] SETI Inst, Mountain View, CA 94043 USA.
[Peeters, E.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Boersma, C (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
EM christiaan.boersma@nasa.gov
RI Boersma, Christiaan/L-7696-2014
OI Boersma, Christiaan/0000-0002-4836-217X
FU NASA's Long Term Space Astrophysics, Astrobiology, Laboratory
Astrophysics; Spitzer Space Telescope Archival Research; NASA's
Astronomy + Physics Research and Analysis (APRA) [NNX07AH02G]; Herschel
Laboratory; Netherlands Organization for Scientific Research (NWO); Ames
Research Center through NASA; European Research Council [246976]
FX This work was supported through NASA's Long Term Space Astrophysics,
Astrobiology, Laboratory Astrophysics, The Spitzer Space Telescope
Archival Research, NASA's Astronomy + Physics Research and Analysis
(APRA; NNX07AH02G), and Herschel Laboratory Astrophysics Programs; the
Netherlands Organization for Scientific Research (NWO) and by an
appointment to the NASA Postdoctoral Program at the Ames Research
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. Studies of interstellar PAHs at Leiden Observatory
are supported through advanced-ERC grant 246976 from the European
Research Council.
NR 38
TC 18
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U1 3
U2 27
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 MAR 1
PY 2011
VL 729
IS 1
AR 64
DI 10.1088/0004-637X/729/1/64
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300064
ER
PT J
AU Das, S
Marriage, TA
Ade, PAR
Aguirre, P
Amiri, M
Appel, JW
Barrientos, LF
Battistelli, ES
Bond, JR
Brown, B
Burger, B
Chervenak, J
Devlin, MJ
Dicker, SR
Doriese, WB
Dunkley, J
Dunner, R
Essinger-Hileman, T
Fisher, RP
Fowler, JW
Hajian, A
Halpern, M
Hasselfield, M
Hernandez-Monteagudo, C
Hilton, GC
Hilton, M
Hincks, AD
Hlozek, R
Huffenberger, KM
Hughes, DH
Hughes, JP
Infante, L
Irwin, KD
Juin, JB
Kaul, M
Klein, J
Kosowsky, A
Lau, JM
Limon, M
Lin, YT
Lupton, RH
Marsden, D
Martocci, K
Mauskopf, P
Menanteau, F
Moodley, K
Moseley, H
Netterfield, CB
Niemack, MD
Nolta, MR
Page, LA
Parker, L
Partridge, B
Reid, B
Sehgal, N
Sherwin, BD
Sievers, J
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Trac, H
Tucker, C
Warne, R
Wollack, E
Zhao, Y
AF Das, Sudeep
Marriage, Tobias A.
Ade, Peter A. R.
Aguirre, Paula
Amiri, Mandana
Appel, John W.
Barrientos, L. Felipe
Battistelli, Elia S.
Bond, John R.
Brown, Ben
Burger, Bryce
Chervenak, Jay
Devlin, Mark J.
Dicker, Simon R.
Doriese, W. Bertrand
Dunkley, Joanna
Duenner, Rolando
Essinger-Hileman, Thomas
Fisher, Ryan P.
Fowler, Joseph W.
Hajian, Amir
Halpern, Mark
Hasselfield, Matthew
Hernandez-Monteagudo, Carlos
Hilton, Gene C.
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Huffenberger, Kevin M.
Hughes, David H.
Hughes, John P.
Infante, Leopoldo
Irwin, Kent D.
Juin, Jean Baptiste
Kaul, Madhuri
Klein, Jeff
Kosowsky, Arthur
Lau, Judy M.
Limon, Michele
Lin, Yen-Ting
Lupton, Robert H.
Marsden, Danica
Martocci, Krista
Mauskopf, Phil
Menanteau, Felipe
Moodley, Kavilan
Moseley, Harvey
Netterfield, Calvin B.
Niemack, Michael D.
Nolta, Michael R.
Page, Lyman A.
Parker, Lucas
Partridge, Bruce
Reid, Beth
Sehgal, Neelima
Sherwin, Blake D.
Sievers, Jon
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Thornton, Robert
Trac, Hy
Tucker, Carole
Warne, Ryan
Wollack, Ed
Zhao, Yue
TI THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE COSMIC MICROWAVE
BACKGROUND POWER SPECTRUM AT 148 AND 218 GHz FROM THE 2008 SOUTHERN
SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations
ID PROBE WMAP OBSERVATIONS; POLE TELESCOPE; BEAM PROFILES; SOURCE COUNTS;
ANISOTROPY; SKY; TEMPERATURE; RADIATION; SIMULATIONS; CONSTRAINTS
AB We present measurements of the cosmic microwave background (CMB) power spectrum made by the Atacama Cosmology Telescope at 148 GHz and 218 GHz, as well as the cross-frequency spectrum between the two channels. Our results clearly show the second through the seventh acoustic peaks in the CMB power spectrum. The measurements of these higher-order peaks provide an additional test of the Lambda CDM cosmological model. At l > 3000, we detect power in excess of the primary anisotropy spectrum of the CMB. At lower multipoles 500 < l < 3000, we find evidence for gravitational lensing of the CMB in the power spectrum at the 2.8 sigma level. We also detect a low level of Galactic dust in our maps, which demonstrates that we can recover known faint, diffuse signals.
C1 [Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Das, Sudeep; Appel, John W.; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Kosowsky, Arthur; Lau, Judy M.; Limon, Michele; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Das, Sudeep; Marriage, Tobias A.; Dunkley, Joanna; Hajian, Amir; Lin, Yen-Ting; Lupton, Robert H.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aguirre, Paula; Barrientos, L. Felipe; Duenner, Rolando; Infante, Leopoldo; Juin, Jean Baptiste; Lin, Yen-Ting] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Bond, John R.; Hajian, Amir; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Brown, Ben] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Marsden, Danica; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Doriese, W. Bertrand; Fowler, Joseph W.; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa.
[Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Hughes, David H.] INAOE, Puebla, Mexico.
[Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Lau, Judy M.; Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
[Kosowsky, Arthur; Martocci, Krista; Switzer, Eric R.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Reid, Beth] Univ Barcelona, ICC, E-08028 Barcelona, Spain.
[Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
[Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Das, S (reprint author), Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Trac,
Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Huffenberger, Kevin/0000-0001-7109-0099; Menanteau,
Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074;
Limon, Michele/0000-0002-5900-2698
FU US National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768]; Princeton University; University of Pennsylvania; Canada
Foundation for Innovation under Compute Canada; Government of Ontario;
Ontario Research Fund-Research Excellence; University of Toronto;
Berkeley Center for Cosmological Physics Fellowship; NASA [NNX08AH30G];
RCUK Fellowship; Rhodes Trust; Natural Science and Engineering Research
Council of Canada (NSERC); NSF [AST-0546035, AST-0606975, PHY-0114422];
FONDAP Centro de Astrofisica; CONICYT; MECESUP; Fundacion Andes; South
African National Research Foundation (NRF); Meraka Institute; South
African Square Kilometer Array (SKA) Project; World Premier
International Research Center Initiative, MEXT, Japan; US Department of
Energy [DE-AC3-76SF00515]; NASA Office of Space Science
FX ACT is on the Chajnantor Science preserve, which was made possible by
the Chilean Comision Nacional de Investigacion Cientifica y Tecnologica.
We are grateful for the assistance we received at various times from the
ALMA, APEX, ASTE, CBI/QUIET, and NANTEN2 groups. The PWV data come from
the public APEX weather Web site. Field operations were based at the Don
Esteban facility run by Astro-Norte. Reed Plimpton and David Jacobson
worked at the telescope during the 2008 season. We thank Norm Jarosik
for support throughout the project. This work was supported by the US
National Science Foundation through awards AST-0408698 for the ACT
project, and PHY-0355328, AST-0707731, and PIRE-0507768. Funding was
also provided by Princeton University and the University of
Pennsylvania. The PIRE program made possible exchanges between Chile,
South Africa, Spain, and the US that enabled this research program.
Computations were performed on the GPC supercomputer at the SciNet HPC
Consortium. SciNet is funded by the Canada Foundation for Innovation
under the auspices of Compute Canada, the Government of Ontario, Ontario
Research Fund-Research Excellence, and the University of Toronto. We
thank the referee for useful comments. S. D. acknowledges support from
the Berkeley Center for Cosmological Physics Fellowship. S. D. thanks
Christian Reichardt and Oliver Zahn for useful discussions. We thank
Bruce Bassett for suggestions on testing lensing in the power spectrum.
S. D., A. H., and T. M. were supported through NASA grant NNX08AH30G. J.
D. acknowledges support from an RCUK Fellowship. R. H. received funding
from the Rhodes Trust. A. D. H. received additional support from a
Natural Science and Engineering Research Council of Canada (NSERC) PGS-D
scholarship. A. K. and B. P. were partially supported through NSF
AST-0546035 and AST-0606975, respectively, for work on ACT. L. I.
acknowledges partial support from FONDAP Centro de Astrofisica. R. D.
was supported by CONICYT, MECESUP, and Fundacion Andes. E. S.
acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to
the Kavli Institute of Cosmological Physics. K. M., M. Hilton, and R. W.
received financial support from the South African National Research
Foundation (NRF), the Meraka Institute via funding for the South African
Centre for High Performance Computing (CHPC), and the South African
Square Kilometer Array (SKA) Project. Y.-T.L. acknowledges support from
the World Premier International Research Center Initiative, MEXT, Japan.
N.S. is supported by the US Department of Energy contract to SLAC no.
DE-AC3-76SF00515. We acknowledge the use of the Legacy Archive for
Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is
provided by the NASA Office of Space Science. The data will be made
public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web
site (http://www.physics.princeton.edu/act/).
NR 57
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U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2011
VL 729
IS 1
AR 62
DI 10.1088/0004-637X/729/1/62
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300062
ER
PT J
AU Fortney, JJ
Ikoma, M
Nettelmann, N
Guillot, T
Marley, MS
AF Fortney, J. J.
Ikoma, M.
Nettelmann, N.
Guillot, T.
Marley, M. S.
TI SELF-CONSISTENT MODEL ATMOSPHERES AND THE COOLING OF THE SOLAR SYSTEM'S
GIANT PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual
(Jupiter, Saturn, Uranus, Neptune); planets and satellites: interiors
ID PROBE MASS-SPECTROMETER; HELIUM FLUID PLANETS; EQUATION-OF-STATE; BROWN
DWARFS; THERMAL STRUCTURE; PHASE-SEPARATION; JUPITERS ATMOSPHERE;
MAGNETIC-FIELDS; JOVIAN PLANETS; T-DWARFS
AB We compute grids of radiative-convective model atmospheres for Jupiter, Saturn, Uranus, and Neptune over a range of intrinsic fluxes and surface gravities. The atmosphere grids serve as an upper boundary condition for models of the thermal evolution of the planets. Unlike previous work, we customize these grids for the specific properties of each planet, including the appropriate chemical abundances and incident fluxes as a function of solar system age. Using these grids, we compute new models of the thermal evolution of the major planets in an attempt to match their measured luminosities at their known ages. Compared to previous work, we find longer cooling times, predominantly due to higher atmospheric opacity at young ages. For all planets, we employ simple "standard" cooling models that feature adiabatic temperature gradients in the interior H/He and water layers, and an initially hot starting point for the calculation of subsequent cooling. For Jupiter, we find a model cooling age similar to 10% longer than previous work, a modest quantitative difference. This may indicate that the hydrogen equation of state used here overestimates the temperatures in the deep interior of the planet. For Saturn, we find a model cooling age similar to 20% longer than previous work. However, an additional energy source, such as that due to helium phase separation, is still clearly needed. For Neptune, unlike in work from the 1980s and 1990s, we match the measured T-eff of the planet with a model that also matches the planet's current gravity field constraints. This is predominantly due to advances in the high-pressure equation of state of water. This may indicate that the planet possesses no barriers to efficient convection in its deep interior. However, for Uranus, our models exacerbate the well-known problem that Uranus is far cooler than calculations predict, which could imply strong barriers to interior convective cooling. The atmosphere grids are published here as tables, so that they may be used by the wider community.
C1 [Fortney, J. J.; Nettelmann, N.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ikoma, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Guillot, T.] CNRS, UMR 6202, Observ Cote Azur, Lab Cassiopee, F-06304 Nice 4, France.
[Marley, M. S.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Fortney, JJ (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM jfortney@ucolick.org
RI Ikoma, Masahiro/B-9915-2012; Marley, Mark/I-4704-2013;
OI Ikoma, Masahiro/0000-0002-5658-5971; Fortney,
Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943
FU NASA [NNX08AU31G]; Alfred P. Sloan Foundation
FX J.J.F. acknowledges the support of NASA Outer Planets Research Program
grant NNX08AU31G and the Alfred P. Sloan Foundation. M. S. M. gratefully
acknowledges the influence of Jim Pollack, who was in the planning
phases of a similar study at the time of his untimely passing. Our
atmospheric modeling is strongly influenced by his work. Referee Gilles
Chabrier provided valuable comments that improved the draft.
NR 96
TC 34
Z9 34
U1 0
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 MAR 1
PY 2011
VL 729
IS 1
AR 32
DI 10.1088/0004-637X/729/1/32
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300032
ER
PT J
AU Kane, SR
Gelino, DM
AF Kane, Stephen R.
Gelino, Dawn M.
TI ON THE INCLINATION DEPENDENCE OF EXOPLANET PHASE SIGNATURES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; techniques: photometric
ID EXTRASOLAR GIANT PLANETS; TAU-BOOTIS-B; REFLECTED STARLIGHT; TRANSITING
PLANET; UPPER LIMIT; LIGHT; PHOTOMETRY; SEPARATION; ROTATION; SPECTRA
AB Improved photometric sensitivity from space-based telescopes has enabled the detection of phase variations for a small sample of hot Jupiters. However, exoplanets in highly eccentric orbits present unique opportunities to study the effects of drastically changing incident flux on the upper atmospheres of giant planets. Here we expand upon previous studies of phase functions for these planets at optical wavelengths by investigating the effects of orbital inclination on the flux ratio as it interacts with the other effects induced by orbital eccentricity. We determine optimal orbital inclinations for maximum flux ratios and combine these calculations with those of projected separation for application to coronagraphic observations. These are applied to several of the known exoplanets which may serve as potential targets in current and future coronagraph experiments.
C1 [Kane, Stephen R.; Gelino, Dawn M.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Kane, SR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, MS 100-22,770 S Wilson Ave, Pasadena, CA 91125 USA.
EM skane@ipac.caltech.edu
RI Kane, Stephen/B-4798-2013
NR 32
TC 14
Z9 14
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2011
VL 729
IS 1
AR 74
DI 10.1088/0004-637X/729/1/74
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300074
ER
PT J
AU LaMassa, SM
Heckman, TM
Ptak, A
Martins, L
Wild, V
Sonnentrucker, P
Hornschemeier, A
AF LaMassa, Stephanie M.
Heckman, T. M.
Ptak, A.
Martins, L.
Wild, V.
Sonnentrucker, P.
Hornschemeier, A.
TI UNCOVERING OBSCURED ACTIVE GALACTIC NUCLEI IN HOMOGENEOUSLY SELECTED
SAMPLES OF SEYFERT 2 GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; infrared: galaxies; X-rays:
galaxies
ID HARD X-RAY; ULTRALUMINOUS INFRARED GALAXIES; XMM-NEWTON OBSERVATIONS;
DIGITAL SKY SURVEY; BLACK-HOLE MASS; COMPTON-THICK; CHANDRA
OBSERVATIONS; EMISSION-LINE; LUMINOSITY FUNCTIONS; STATISTICAL-METHODS
AB We have analyzed archival Chandra and XMM-Newton data for two nearly complete homogeneously selected samples of type 2 Seyfert galaxies (Sy2s). These samples were selected based on intrinsic active galactic nuclei (AGNs) flux proxies: a mid-infrared (MIR) sample from the original IRAS 12 mu m survey and an optical ([OIII]lambda 5007 flux limited) sample from the Sloan Digital Sky Survey, providing a total of 45 Sy2s. As the MIR and [OIII] fluxes are largely unaffected by AGN obscuration, these samples can present an unbiased estimate of the Compton-thick (column density N-H > 10(24) cm(-2)) subpopulation. We find that the majority of this combined sample are likely heavily obscured, as evidenced by the 2-10 keV X-ray attenuation (normalized by intrinsic flux diagnostics) and the large Fe K alpha equivalent widths (several hundred eV to over 1 keV). A wide range of these obscuration diagnostics is present, showing a continuum of column densities, rather than a clear segregation into Compton-thick and Compton-thin sub-populations. We find that, in several instances, the fitted column densities severely underrepresent the attenuation implied by these obscuration diagnostics, indicating that simple X-ray models may not always recover the intrinsic absorption. We compared AGNs and host galaxy properties, such as intrinsic luminosity, central black hole mass, accretion rate, and star formation rate with obscuration diagnostics. No convincing evidence exists to link obscured sources with unique host galaxy populations from their less absorbed counterparts. Finally, we estimate that a majority of these Seyfert 2s will be detectable in the 10-40 keV range by the future NuSTAR mission, which would confirm whether these heavily absorbed sources are indeed Compton-thick.
C1 [LaMassa, Stephanie M.; Heckman, T. M.; Sonnentrucker, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ptak, A.; Hornschemeier, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Martins, L.] Univ Cruzeiro Sul, NAT, Sao Paulo, Brazil.
[Wild, V.] Inst Astrophys Paris, F-75014 Paris, France.
RP LaMassa, SM (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RI Martins, Lucimara/K-5158-2012; 7, INCT/H-6207-2013; Astrofisica,
Inct/H-9455-2013
OI Martins, Lucimara/0000-0001-6505-5190;
FU Spitzer grant [RSA1287640]; [10-ADAP10-0167]
FX This work was supported by grant 10-ADAP10-0167 and Spitzer grant
RSA1287640. The authors thank the anonymous referee whose comments and
suggestions improved the manuscript. This research has made use of data
obtained from the High Energy Astrophysics Science Archive Research
Center (HEASARC), provided by NASA's Goddard Space Flight Center.
NR 84
TC 28
Z9 28
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2011
VL 729
IS 1
AR 52
DI 10.1088/0004-637X/729/1/52
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300052
ER
PT J
AU Matsuo, T
Traub, WA
Hattori, M
Tamura, M
AF Matsuo, Taro
Traub, Wesley A.
Hattori, Makoto
Tamura, Motohide
TI A NEW CONCEPT FOR DIRECT IMAGING AND SPECTRAL CHARACTERIZATION OF
EXOPLANETS IN MULTI-PLANET SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; techniques: interferometric
ID INTERFEROMETER; LIFE; STAR
AB We present a novel method for direct detection and characterization of exoplanets from space. This method uses four collecting telescopes, combined with phase chopping and a spectrometer, with observations on only a few baselines rather than on a continuously rotated baseline. Focusing on the contiguous wavelength spectra of typical exoplanets, the (u, v) plane can be simultaneously and uniformly filled by recording the spectrally resolved signal. This concept allows us to perfectly remove speckles from reconstructed images. For a target comprising a star and multiple planets, observations on three baselines are sufficient to extract the position and spectrum of each planet. Our simulations show that this new method allows us to detect an analog Earth around a Sun-like star at 10 pc and to acquire its spectrum over the wavelength range from 8 to 19 mu m with a high spectral resolution of 100. This method allows us to fully characterize an analog Earth and to similarly characterize each planet in multi-planet systems.
C1 [Matsuo, Taro; Tamura, Motohide] Natl Astron Observ Japan, Tokyo 1810015, Japan.
[Traub, Wesley A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hattori, Makoto] Tohoku Univ, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Matsuo, T (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Tokyo 1810015, Japan.
EM taro.matsuo@nao.ac.jp
NR 21
TC 0
Z9 0
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2011
VL 729
IS 1
AR 50
DI 10.1088/0004-637X/729/1/50
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300050
ER
PT J
AU Williams, BJ
Borkowski, KJ
Reynolds, SP
Ghavamian, P
Raymond, JC
Long, KS
Blair, WP
Sankrit, R
Smith, RC
Points, S
Winkler, PF
Hendrick, SP
AF Williams, Brian J.
Borkowski, Kazimierz J.
Reynolds, Stephen P.
Ghavamian, Parviz
Raymond, John C.
Long, Knox S.
Blair, William P.
Sankrit, Ravi
Smith, R. Chris
Points, Sean
Winkler, P. Frank
Hendrick, Sean P.
TI DUSTY BLAST WAVES OF TWO YOUNG LARGE MAGELLANIC CLOUD SUPERNOVA
REMNANTS: CONSTRAINTS ON POST-SHOCK COMPRESSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: supernova remnants; Magellanic Clouds
ID GRAIN-SIZE DISTRIBUTIONS; SPITZER OBSERVATIONS; RED CLUMP; EMISSION;
DESTRUCTION; PHYSICS; ACCELERATION; SPECTRA; PLASMA; LINES
AB We present results from mid-IR spectroscopic observations of two young supernova remnants (SNRs) in the Large Magellanic Cloud made with the Spitzer Space Telescope. We imaged SNRs B0509-67.5 and B0519-69.0 with Spitzer in 2005, and follow-up spectroscopy presented here confirms the presence of warm, shock-heated dust, with no lines present in the spectrum. We use model fits to Spitzer Infrared Spectrograph (IRS) data to estimate the density of the post-shock gas. Both remnants show asymmetries in the infrared images, and we interpret bright spots as places where the forward shock is running into material that is several times denser than elsewhere. The densities we infer for these objects depend on the grain composition assumed, and we explore the effects of differing grain porosity on the model fits. We also analyze archival XMM-Newton RGS spectroscopic data, where both SNRs show strong lines of both Fe and Si, coming from ejecta, as well as strong O lines, which may come from ejecta or shocked ambient medium. We use model fits to IRS spectra to predict X-ray O line strengths for various grain models and values of the shock compression ratio. For 0509-67.5, we find that compact (solid) grain models require nearly all O lines in X-ray spectra to originate in reverse-shocked ejecta. Porous dust grains would lower the strength of ejecta lines relative to those arising in the shocked ambient medium. In 0519-69.0, we find significant evidence for a higher than standard compression ratio of 12, implying efficient cosmic-ray acceleration by the blast wave. A compact grain model is favored over porous grain models. We find that the dust-to-gas mass ratio of the ambient medium is significantly lower than what is expected in the interstellar medium.
C1 [Williams, Brian J.; Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Ghavamian, Parviz; Long, Knox S.] STScI, Baltimore, MD 21218 USA.
[Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Smith, R. Chris; Points, Sean] CTIO, La Serena, Chile.
[Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Hendrick, Sean P.] Millersville Univ Pennsylvania, Dept Phys, Millersville, PA 17551 USA.
RP Williams, BJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
EM bjwilli2@ncsu.edu
FU Spitzer Guest Observer Grant [RSA 1328682]
FX We thank John Blondin for providing the VH-1 hydrodynamics code and for
useful discussions on interpretation, and the anonymous referee for many
useful comments which improved the paper. We acknowledge support from
Spitzer Guest Observer Grant RSA 1328682.
NR 52
TC 21
Z9 21
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2011
VL 729
IS 1
AR 65
DI 10.1088/0004-637X/729/1/65
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300065
ER
PT J
AU Basu, S
Grundahl, F
Stello, D
Kallinger, T
Hekker, S
Mosser, B
Garcia, RA
Mathur, S
Brogaard, K
Bruntt, H
Chaplin, WJ
Gai, N
Elsworth, Y
Esch, L
Ballot, J
Bedding, TR
Gruberbauer, M
Huber, D
Miglio, A
Yildiz, M
Kjeldsen, H
Christensen-Dalsgaard, J
Gilliland, RL
Fanelli, MM
Ibrahim, KA
Smith, JC
AF Basu, Sarbani
Grundahl, Frank
Stello, Dennis
Kallinger, Thomas
Hekker, Saskia
Mosser, Benoit
Garcia, Rafael A.
Mathur, Savita
Brogaard, Karsten
Bruntt, Hans
Chaplin, William J.
Gai, Ning
Elsworth, Yvonne
Esch, Lisa
Ballot, Jerome
Bedding, Timothy R.
Gruberbauer, Michael
Huber, Daniel
Miglio, Andrea
Yildiz, Mutlu
Kjeldsen, Hans
Christensen-Dalsgaard, Jorgen
Gilliland, Ronald L.
Fanelli, Michael M.
Ibrahim, Khadeejah A.
Smith, Jeffrey C.
TI SOUNDING OPEN CLUSTERS: ASTEROSEISMIC CONSTRAINTS FROM KEPLER ON THE
PROPERTIES OF NGC 6791 AND NGC 6819
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE open clusters and associations: individual (NGC 6819, NGC 6791); stars:
fundamental parameters; stars: interiors; stars: oscillations
ID SOLAR-LIKE OSCILLATIONS; RED GIANTS; RADIUS DETERMINATION; STARS;
PHOTOMETRY; NGC-6791; PARAMETERS; ISOCHRONES; EVOLUTION; OLD
AB We present initial results on some of the properties of open clusters NGC 6791 and NGC 6819 derived from asteroseismic data obtained by NASA's Kepler mission. In addition to estimating the mass, radius, and log g of stars on the red giant branch (RGB) of these clusters, we estimate the distance to the clusters and their ages. Our model-independent estimate of the distance modulus of NGC 6791 is (m - M)(0) = 13.11 +/- 0.06. We find (m - M)(0) = 11.85 +/- 0.05 for NGC 6819. The average mass of stars on the RGB of NGC 6791 is 1.20 +/- 0.01 M-circle dot, while that of NGC 6819 is 1.68 +/- 0.03 M-circle dot. It should be noted that we do not have data that cover the entire RGB and the actual mass will be somewhat lower. We have determined model-dependent estimates of ages of these clusters. We find ages between 6.8 and 8.6 Gyr for NGC 6791, however, most sets of models give ages around 7 Gyr. We obtain ages between 2 and 2.4 Gyr for NGC 6819.
C1 [Basu, Sarbani; Esch, Lisa] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Grundahl, Frank; Brogaard, Karsten; Bruntt, Hans; Kjeldsen, Hans; Christensen-Dalsgaard, Jorgen] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Stello, Dennis; Bedding, Timothy R.; Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Kallinger, Thomas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Kallinger, Thomas] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Hekker, Saskia; Chaplin, William J.; Elsworth, Yvonne] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Mosser, Benoit] Univ Paris 07, Observ Paris, Univ Paris 06, LESIA,CNRS, F-92195 Meudon, France.
[Garcia, Rafael A.] Univ Paris 07, CEA DSM CNRS, Lab AIM, IRFU SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Mathur, Savita] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Gai, Ning] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China.
[Ballot, Jerome] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France.
[Gruberbauer, Michael] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Miglio, Andrea] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Yildiz, Mutlu] Ege Univ, Dept Astron & Space Sci, TR-35100 Izmir, Turkey.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Fanelli, Michael M.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Ibrahim, Khadeejah A.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Smith, Jeffrey C.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Basu, S (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA.
EM sarbani.basu@yale.edu
RI Ballot, Jerome/G-1019-2010;
OI Kallinger, Thomas/0000-0003-3627-2561; Brogaard,
Karsten/0000-0003-2001-0276; Bedding, Timothy/0000-0001-5943-1460;
Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776
FU NASA's Science Mission Directorate
FX Funding for the Kepler mission is provided by NASA's Science Mission
Directorate. The authors wish to thank the entire Kepler team, without
whom these results would not be possible. We also thank all funding
councils and agencies that have supported the activities of Working
Group 2 of the Kepler Asteroseismic Science Consortium.
NR 42
TC 70
Z9 70
U1 1
U2 7
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 MAR 1
PY 2011
VL 729
IS 1
AR L10
DI 10.1088/2041-8205/729/1/L10
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 719HI
UT WOS:000287194100010
ER
PT J
AU Susskind, J
Blaisdell, JM
Iredell, L
Keita, F
AF Susskind, Joel
Blaisdell, John M.
Iredell, Lena
Keita, Fricky
TI Improved Temperature Sounding and Quality Control Methodology Using
AIRS/AMSU Data: The AIRS Science Team Version 5 Retrieval Algorithm
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Atmospheric Infrared Sounder/Advanced Microwave Sounding Unit
(AIRS/AMSU); cloud-cleared radiances; error estimates; high
spectral-resolution infrared sounders; infrared sounding in cloudy
conditions; retrieval methodology
ID CLOUDY ATMOSPHERES; PARAMETERS; PRODUCTS; SURFACE
AB This paper describes the Atmospheric Infrared Sounder (AIRS) Science Team Version 5 retrieval algorithm in terms of its three most significant improvements over the methodology used in the AIRS Science Team Version 4 retrieval algorithm: the use of AIRS clear-column radiances in the entire 4.3-mu m CO2 absorption band in the retrieval of temperature profiles T (p) during both day and night, with tropospheric sounding of 15-mu m CO2 observations now being used primarily in the generation of clear-column radiances (R) over cap (i) for all channels; development of a new methodology to provide accurate case-by-case error estimates for retrieved geophysical parameters and for channel-by-channel clear column radiances and their use in a new approach for quality control; and an approach to provide AIRS soundings in partially cloudy conditions that does not require use of any microwave data. This new AIRS-only sounding methodology, referred to as AIRS Version 5 AO, was developed as a backup to AIRS Version 5 should the Advanced Microwave Sounding Unit (AMSU)-A instrument fail. Results are shown that compare the relative performance of the AIRS Version 4, Version 5, and Version 5 AO. Results using Version 5 retrievals in conjunction with different quality control thresholds are also shown for a recent period to demonstrate that empirical coefficients continue to be applicable in later time periods. The Goddard Data and Information Services Center (DISC) is now generating and distributing products derived using the AIRS Science Team Version 5 retrieval algorithm. This paper describes the quality control flags contained in the DISC AIRS/AMSU retrieval products and their intended use for scientific purposes.
C1 [Susskind, Joel; Blaisdell, John M.; Iredell, Lena; Keita, Fricky] NASA, Goddard Space Flight Ctr, Sci Applicat Int Corp, Greenbelt, MD 20771 USA.
RP Susskind, J (reprint author), NASA, Goddard Space Flight Ctr, Sci Applicat Int Corp, Greenbelt, MD 20771 USA.
EM Joel.Susskind-1@nasa.gov; John.Blaisdell@nasa.gov; Lena.Iredell@nasa.gov
NR 19
TC 63
Z9 63
U1 0
U2 17
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 MAR
PY 2011
VL 49
IS 3
BP 883
EP 907
DI 10.1109/TGRS.2010.2070508
PG 25
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 725PN
UT WOS:000287658000001
ER
PT J
AU Mishchenko, MI
Menguc, MP
Rothman, LS
AF Mishchenko, Michael I.
Menguec, M. Pinar
Rothman, Laurence S.
TI Van de Hulst Light-Scattering Award
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Menguec, M. Pinar] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM crmim2@gmail.com
RI Menguc, Pinar/O-3114-2013; Mishchenko, Michael/D-4426-2012;
OI Rothman, Laurence/0000-0002-3837-4847
NR 0
TC 0
Z9 0
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2011
VL 112
IS 4
SI SI
BP 559
EP 559
DI 10.1016/j.jqsrt.2010.11.018
PG 1
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 725VO
UT WOS:000287675000001
ER
PT J
AU Davis, AB
Sanchez, R
AF Davis, Anthony B.
Sanchez, Richard
TI Two Truly Special Sessions at the 2009 International Conference on
Mathematics and Computational Methods (M&C 2009): Transport ... Across
Disciplinary Divides
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
ID MISSION
C1 [Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Sanchez, Richard] Ctr Etud Nucl Saclay, Commissariat Energie Atom & Energies Alternat, Gif Sur Yvette, France.
RP Davis, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-237, Pasadena, CA 91125 USA.
EM Anthony.B.Davis@jpl.nasa.gov
NR 28
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 MAR
PY 2011
VL 112
IS 4
SI SI
BP 560
EP 565
DI 10.1016/j.jqsrt.2010.11.014
PG 6
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 725VO
UT WOS:000287675000002
ER
PT J
AU Davis, AB
Mineev-Weinstein, MB
AF Davis, Anthony B.
Mineev-Weinstein, Mark B.
TI Radiation propagation in random media: From positive to negative
correlations in high-frequency fluctuations
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article; Proceedings Paper
CT International Conference on Advances in Mathematics, Computational
Methods and Reactor Physics
CY MAY 03-07, 2009
CL Saratoga Springs, NY
SP Amer Nucl Soc
DE Multi-dimensional radiation transport; Stochastic media; Non-exponential
transmission laws; Clustering/anti-clustering material particles;
Negative spatial correlations
ID BOUNDARY-LAYER CLOUDS; INDEPENDENT COLUMN APPROXIMATION; CHORD LENGTH
DISTRIBUTIONS; THICK MULTIFRACTAL CLOUDS; DROP-SIZE VARIABILITY;
AVERAGED SOLAR FLUXES; INHOMOGENEOUS CLOUDS; PARTICLE-TRANSPORT; OPTICAL
MEDIA; BREAST-TISSUE
AB We survey research on radiation propagation or ballistic particle motion through media with randomly variable material density, and we investigate the topic with an emphasis on very high spatial frequencies. Our new results are based on a specific variability model consisting of a zero-mean Gaussian scaling noise riding on a constant value that is large enough with respect to the amplitude of the noise to yield overwhelmingly non-negative density. We first generalize known results about sub-exponential transmission from regular functions, which are almost everywhere continuous, to merely "measurable" ones, which are almost everywhere discontinuous (akin to statistically stationary noises), with positively correlated fluctuations. We then use the generalized measure-theoretic formulation to address negatively correlated stochastic media without leaving the framework of conventional (continuum-limit) transport theory. We thus resolve a controversy about recent claims that only discrete-point process approaches can accommodate negative correlations, i.e., anti-clustering of the material particles. We obtain in this case the predicted super-exponential behavior, but it is rather weak. Physically, and much like the alternative discrete-point process approach, the new model applies most naturally to scales commensurate with the inter-particle distance in the material, i.e., when the notion of particle density breaks down due to Poissonian-or maybe not-so-Poissonian-number-count fluctuations occur in the sample volume. At the same time, the noisy structure must prevail up to scales commensurate with the mean-free-path to be of practical significance. Possible applications are discussed. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mineev-Weinstein, Mark B.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Davis, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Anthony.B.Davis@jpl.nasa.gov
NR 70
TC 13
Z9 13
U1 1
U2 4
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 MAR
PY 2011
VL 112
IS 4
SI SI
BP 632
EP 645
DI 10.1016/j.jqsrt.2010.10.001
PG 14
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 725VO
UT WOS:000287675000007
ER
PT J
AU Mishchenko, MI
Tishkovets, VP
Travis, LD
Cairns, B
Dlugach, JM
Liu, L
Rosenbush, VK
Kiselev, NN
AF Mishchenko, Michael I.
Tishkovets, Victor P.
Travis, Larry D.
Cairns, Brian
Dlugach, Janna M.
Liu, Li
Rosenbush, Vera K.
Kiselev, Nikolai N.
TI Electromagnetic scattering by a morphologically complex object:
Fundamental concepts and common misconceptions
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article; Proceedings Paper
CT International Conference on Advances in Mathematics, Computational
Methods and Reactor Physics
CY MAY 03-07, 2009
CL Saratoga Springs, NY
SP Amer Nucl Soc
DE Macroscopic Maxwell equations; Electromagnetic scattering; Multiple
scattering; Coherent backscattering; Radiative transfer
ID DISCRETE DIPOLE APPROXIMATION; RADIATIVE-TRANSFER EQUATION; RANDOM
PARTICULATE MEDIA; SOLAR-SYSTEM OBJECTS; LIGHT-SCATTERING; COHERENT
BACKSCATTERING; MULTIPLE-SCATTERING; WEAK-LOCALIZATION; ABSORBING
MEDIUM; SINGLE-SCATTERING
AB Following Keller (Proc Symp Appl Math 1962;13:227-46), we classify all theoretical treatments of electromagnetic scattering by a morphologically complex object into first-principle (or "honest" in Keller's terminology) and phenomenological (or "dishonest") categories. This helps us identify, analyze, and dispel several profound misconceptions widespread in the discipline of electromagnetic scattering by solitary particles and discrete random media. Our goal is not to call for a complete renunciation of phenomenological approaches but rather to encourage a critical and careful evaluation of their actual origin, virtues, and limitations. In other words, we do not intend to deter creative thinking in terms of phenomenological short-cuts, but we do want to raise awareness when we stray (often for practical reasons) from the fundamentals. The main results and conclusions are illustrated by numerically-exact data based on direct numerical solutions of the macroscopic Maxwell equations. Published by Elsevier Ltd.
C1 [Mishchenko, Michael I.; Travis, Larry D.; Cairns, Brian; Liu, Li] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Tishkovets, Victor P.] Inst Radio Astron NASU, UA-61002 Kharkov, Ukraine.
[Dlugach, Janna M.; Rosenbush, Vera K.; Kiselev, Nikolai N.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM crmim2@gmail.com
RI Mishchenko, Michael/D-4426-2012;
OI Cairns, Brian/0000-0002-1980-1022
NR 113
TC 43
Z9 44
U1 2
U2 10
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 MAR
PY 2011
VL 112
IS 4
SI SI
BP 671
EP 692
DI 10.1016/j.jqsrt.2010.03.016
PG 22
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 725VO
UT WOS:000287675000010
ER
PT J
AU Schull, MA
Knyazikhin, Y
Xu, L
Samanta, A
Carmona, PL
Lepine, L
Jenkins, JP
Ganguly, S
Myneni, RB
AF Schull, M. A.
Knyazikhin, Y.
Xu, L.
Samanta, A.
Carmona, P. L.
Lepine, L.
Jenkins, J. P.
Ganguly, S.
Myneni, R. B.
TI Canopy spectral invariants, Part 2: Application to classification of
forest types from hyperspectral data
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article; Proceedings Paper
CT International Conference on Advances in Mathematics, Computational
Methods and Reactor Physics
CY MAY 03-07, 2009
CL Saratoga Springs, NY
SP Amer Nucl Soc
DE Spectral invariants; Vegetation structure; Ecosystem; Scaling;
Scattering albedo; Hyperspectral data; Radiative transfer
ID NET PRIMARY PRODUCTION; LEAF-AREA INDEX; IMAGING SPECTROSCOPY;
VEGETATION CANOPIES; ENDMEMBER SELECTION; RADIATIVE-TRANSFER;
SOLAR-RADIATION; SHOOT STRUCTURE; WATER-CONTENT; SCOTS PINE
AB Many studies have been conducted to demonstrate the ability of hyperspectral data to discriminate plant dominant species. Most of them have employed the use of empirically based techniques, which are site specific, requires some initial training based on characteristics of known leaf and/or canopy spectra and therefore may not be extendable to operational use or adapted to changing or unknown land cover. In this paper we propose a physically based approach for separation of dominant forest type using hyperspectral data. The radiative transfer theory of canopy spectral invariants underlies the approach, which facilitates parameterization of the canopy reflectance in terms of the leaf spectral scattering and two spectrally invariant and structurally varying variables-recollision and directional escape probabilities. The methodology is based on the idea of retrieving spectrally invariant parameters from hyperspectral data first, and then relating their values to structural characteristics of three-dimensional canopy structure. Theoretical and empirical analyses of ground and airborne data acquired by Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) over two sites in New England, USA, suggest that the canopy spectral invariants convey information about canopy structure at both the macro- and micro-scales. The total escape probability (one minus recollision probability) varies as a power function with the exponent related to the number of nested hierarchical levels present in the pixel. Its base is a geometrical mean of the local total escape probabilities and accounts for the cumulative effect of canopy structure over a wide range of scales. The ratio of the directional to the total escape probability becomes independent of the number of hierarchical levels and is a function of the canopy structure at the macro-scale such as tree spatial distribution, crown shape and size, within-crown foliage density and ground cover. These properties allow for the natural separation of dominant forest classes based on the location of points on the total escape probability vs the ratio log-log plane. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Schull, M. A.; Knyazikhin, Y.; Xu, L.; Samanta, A.; Myneni, R. B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Carmona, P. L.] Univ Jaume 1, Dept Lenguajes & Sistemas Informat, Castellon De La Plana 12071, Spain.
[Lepine, L.; Jenkins, J. P.] Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03829 USA.
[Ganguly, S.] NASA, Ames Res Ctr, Bay Area, Environm Res Inst, Moffett Field, CA 94035 USA.
RP Schull, MA (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA.
EM schull@bu.edu
RI Xu, Liang/D-1247-2013; ganguly, sangram/B-5108-2010; Myneni,
Ranga/F-5129-2012;
OI Lepine, Lucie/0000-0003-1028-2534
NR 54
TC 18
Z9 18
U1 1
U2 15
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 MAR
PY 2011
VL 112
IS 4
SI SI
BP 736
EP 750
DI 10.1016/j.jqsrt.2010.06.004
PG 15
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 725VO
UT WOS:000287675000014
ER
PT J
AU Mesnick, SL
Taylor, BL
Archer, FI
Martien, KK
Trevino, SE
Hancock-Hanser, BL
Medina, SCM
Pease, VL
Robertson, KM
Straley, JM
Baird, RW
Calambokidis, J
Schorr, GS
Wade, P
Burkanov, V
Lunsford, CR
Rendell, L
Morin, PA
AF Mesnick, Sarah L.
Taylor, Barbara L.
Archer, Frederick I.
Martien, Karen K.
Trevino, Sergio Escorza
Hancock-Hanser, Brittany L.
Moreno Medina, Sandra Carolina
Pease, Victoria L.
Robertson, Kelly M.
Straley, Janice M.
Baird, Robin W.
Calambokidis, John
Schorr, Gregory S.
Wade, Paul
Burkanov, Vladimir
Lunsford, Chris R.
Rendell, Luke
Morin, Phillip A.
TI Sperm whale population structure in the eastern and central North
Pacific inferred by the use of single-nucleotide polymorphisms,
microsatellites and mitochondrial DNA
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE conservation; Physeter macrocephalus; population structure;
single-nucleotide polymorphism; sperm whale
ID PHYSETER-MACROCEPHALUS; GENETIC DIFFERENTIATION; SOCIAL-ORGANIZATION;
MAXIMUM-LIKELIHOOD; GENOTYPING ERRORS; STATISTICAL POWER; F-STATISTICS;
VOCAL CLANS; G(ST); SNPS
AB We use mitochondrial DNA (mtDNA) (400 bp), six microsatellites and 36 single-nucleotide polymorphisms (SNPs), 20 of which were linked, to investigate population structure of sperm whales (Physeter macrocephalus) in the eastern and central North Pacific. SNP markers, reproducible across technologies and laboratories, are ideal for long-term studies of globally distributed species such as sperm whales, a species of conservation concern because of both historical and contemporary impacts. We estimate genetic differentiation among three strata in the temperate to tropical waters where females are found: California Current, Hawaigravei and the eastern tropical Pacific. We then consider how males on sub-Arctic foraging grounds assign to these strata. The California Current stratum was differentiated from both the other strata (P < 0.05) for mtDNA, microsatellites and SNPs, suggesting that the region supports a demographically independent population and providing the first indication that males may exhibit reproductive philopatry. Comparisons between the Hawaigravei stratum and the eastern tropical Pacific stratum are not conclusive at this time. Comparisons with Alaska males were statistically significant, or nearly so, from all three strata and individuals showed mixed assignment to, and few exclusions from, the three potential source strata, suggesting widespread origin of males on sub-Arctic feeding grounds. We show that SNPs have sufficient power to detect population structure even when genetic differentiation is low. There is a need for better analytical methods for SNPs, especially when linked SNPs are used, but SNPs appear to be a valuable marker for long-term studies of globally dispersed and highly mobile species.
C1 [Mesnick, Sarah L.; Taylor, Barbara L.; Archer, Frederick I.; Martien, Karen K.; Hancock-Hanser, Brittany L.; Pease, Victoria L.; Robertson, Kelly M.; Morin, Phillip A.] SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, La Jolla, CA 92037 USA.
[Mesnick, Sarah L.; Morin, Phillip A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Trevino, Sergio Escorza] Calif State Univ Los Angeles, Dept Biol Sci, Los Angeles, CA 90032 USA.
[Moreno Medina, Sandra Carolina] Univ Autonoma Baja California, Lab Ecol Mol, Ensenada 22800, Baja California, Mexico.
[Straley, Janice M.] Univ Alaska SE, Sitka, AK 99835 USA.
[Baird, Robin W.; Calambokidis, John; Schorr, Gregory S.] Cascadia Res Collect, Olympia, WA 98501 USA.
[Wade, Paul; Burkanov, Vladimir] Natl Marine Fisheries Serv, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, Seattle, WA 98115 USA.
[Burkanov, Vladimir] RAS, FEB, Kamchatka Branch, Pacific Geophys Inst, Petropavlovsk Kamchatski, Russia.
[Lunsford, Chris R.] Natl Marine Fisheries Serv, Auke Bay Lab, Alaska Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, Juneau, AK 99801 USA.
[Rendell, Luke] Sch Biol, St Andrews KY16 9TS, Fife, Scotland.
RP Mesnick, SL (reprint author), SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, 3333 N Torrey Pines Court, La Jolla, CA 92037 USA.
EM sarah.mesnick@noaa.gov
RI Rendell, Luke/G-2594-2010
OI Rendell, Luke/0000-0002-1121-9142
FU Southwest Fisheries Science Center (SWFSC), Southwest Regional Office;
Alaska Regional Office of the National Marine Fisheries Service (NMFS);
National Oceanic and Atmospheric Administration (NOAA); U.S. Marine
Mammal Commission
FX Research was funded by the Southwest Fisheries Science Center (SWFSC),
Southwest Regional Office and Alaska Regional Office of the National
Marine Fisheries Service (NMFS), National Oceanic and Atmospheric
Administration (NOAA), and the U.S. Marine Mammal Commission. We are
thankful for expertise of tissue archivist Gabriella Serra-Valente and
the laboratory expertise of John Hyde, Aviva Rosenberg, Becky Nachenberg
and Karine Viaud. Andy Dizon provided initial support, Dan Prosperi
provided valuable guidance in database management, Rich Cosgrove
provided the maps and Henry Orr improved the figures. Sample collection
was carried out by the SWFSC under National Marine Fisheries Service
Permits 1029/689424, 774-1437 and 774-1714 as required by the Marine
Mammal Protection Act and Endangered Species Act. Bill Perrin, Aimee
Lang, John Hyde, Nikki Volmer, Susan Chivers, David Paetkau and three
anonymous reviewers provided valuable comments that improved the
manuscript. Collection of samples involved many people, from many
institutions. Our gratitude goes to the command and crew of NOAA Ships
David Starr Jordan, McArthur, McArthur II, the UNOLS vessel Endeavor,
and to SWFSC Chief Scientists: Lisa Ballance, Jay Barlow, Susan Chivers,
Karin Forney, Tim Gerrodette and Rick LeDuc. The skill of several expert
marine mammal observers made it possible for us to obtain samples on
these cruises, among them: Robert Pitman, Juan Carlos Salinas, Jim
Cotton, Suzanne Yin and Erin LaBreque. We are grateful to the many
scientists and institutions that have contributed valuable samples to
this project: Alaska SeaLife Center; Diane Gendron, Centro
Interdisciplinario de Ciencias Marinas, Instituto Politecnico Nacional;
Lance Barrett Lennard, Cowan Vertebrate Museum, University of British
Columbia; Jenny Christal, Dalhousie University; Kristine Sowl, Izembek
National Wildlife Refuge, U.S. Fish and Wildlife Service; Jim Dines, Los
Angeles County Museum of Natural History; Moss Landing Marine
Laboratories; John Durban, National Marine Mammal Lab, Alaska Fisheries
Science Center, NMFS, NOAA; Craig Matkin, North Gulf Oceaninc Society;
Jan Hodder, Oregon Institute of Marine Biology, University of Oregon;
Daniel Palacios, Oregon State University-Corvallis and now at SWFSC,
NMFS, NOAA; Pacific Islands Fisheries Science Center, NMFS, NOAA; Santa
Barbara Museum of Natural History; Nancy Black; Southwest Region Fishery
Observer Program; The Marine Mammal Center; Jorge Urban-Ramirez,
Universidad Autonoma de Baja California Sur; Link Olson, University of
Alaska Museum; Kate Wynne, University of Alaska, Fairbanks; University
of British Columbia.
NR 99
TC 30
Z9 33
U1 4
U2 55
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1755-098X
J9 MOL ECOL RESOUR
JI Mol. Ecol. Resour.
PD MAR
PY 2011
VL 11
SU 1
BP 278
EP 298
DI 10.1111/j.1755-0998.2010.02973.x
PG 21
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 723CZ
UT WOS:000287485100024
PM 21429181
ER
PT J
AU Woods, PM
Oliveira, JM
Kemper, F
van Loon, JT
Sargent, BA
Matsuura, M
Szczerba, R
Volk, K
Zijlstra, AA
Sloan, GC
Lagadec, E
McDonald, I
Jones, O
Gorjian, V
Kraemer, KE
Gielen, C
Meixner, M
Blum, RD
Sewilo, M
Riebel, D
Shiao, B
Chen, CHR
Boyer, ML
Indebetouw, R
Antoniou, V
Bernard, JP
Cohen, M
Dijkstra, C
Galametz, M
Galliano, F
Gordon, KD
Harris, J
Hony, S
Hora, JL
Kawamura, A
Lawton, B
Leisenring, JM
Madden, S
Marengo, M
McGuire, C
Mulia, AJ
O'Halloran, B
Olsen, K
Paladini, R
Paradis, D
Reach, WT
Rubin, D
Sandstrom, K
Soszynski, I
Speck, AK
Srinivasan, S
Tielens, AGGM
van Aarle, E
Van Dyk, SD
Van Winckel, H
Vijh, UP
Whitney, B
Wilkins, AN
AF Woods, Paul M.
Oliveira, J. M.
Kemper, F.
van Loon, J. Th.
Sargent, B. A.
Matsuura, M.
Szczerba, R.
Volk, K.
Zijlstra, A. A.
Sloan, G. C.
Lagadec, E.
McDonald, I.
Jones, O.
Gorjian, V.
Kraemer, K. E.
Gielen, C.
Meixner, M.
Blum, R. D.
Sewilo, M.
Riebel, D.
Shiao, B.
Chen, C. -H. R.
Boyer, M. L.
Indebetouw, R.
Antoniou, V.
Bernard, J. -P.
Cohen, M.
Dijkstra, C.
Galametz, M.
Galliano, F.
Gordon, Karl D.
Harris, J.
Hony, S.
Hora, J. L.
Kawamura, A.
Lawton, B.
Leisenring, J. M.
Madden, S.
Marengo, M.
McGuire, C.
Mulia, A. J.
O'Halloran, B.
Olsen, K.
Paladini, R.
Paradis, D.
Reach, W. T.
Rubin, D.
Sandstrom, K.
Soszynski, I.
Speck, A. K.
Srinivasan, S.
Tielens, A. G. G. M.
van Aarle, E.
Van Dyk, S. D.
Van Winckel, H.
Vijh, Uma P.
Whitney, B.
Wilkins, A. N.
TI The SAGE-Spec Spitzer Legacy programme: the life-cycle of dust and gas
in the Large Magellanic Cloud - Point source classification I
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: spectroscopic; surveys; galaxies: individual: LMC;
Magellanic Clouds; infrared: galaxies; infrared: stars
ID ASYMPTOTIC GIANT BRANCH; YOUNG STELLAR OBJECTS; LONG-PERIOD VARIABLES;
POST-AGB STARS; GRAVITATIONAL LENSING EXPERIMENT.; CORONAE-BOREALIS
STARS; OGLE-III CATALOG; MU-M SOURCES; EXTREME CARBON STARS; WOLF-RAYET
STARS
AB We present the classification of 197 point sources observed with the Infrared Spectrograph in the SAGE-Spec Legacy programme on the Spitzer Space Telescope. We introduce a decision-tree method of object classification based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information, which is used to classify the SAGE-Spec sample of point sources. The decision tree has a broad application to mid-infrared spectroscopic surveys, where supporting photometry and variability information are available. We use these classifications to make deductions about the stellar populations of the Large Magellanic Cloud and the success of photometric classification methods. We find 90 asymptotic giant branch (AGB) stars, 29 young stellar objects, 23 post-AGB objects, 19 red supergiants, eight stellar photospheres, seven background galaxies, seven planetary nebulae, two H II regions and 12 other objects, seven of which remain unclassified.
C1 [Woods, Paul M.; Kemper, F.; Zijlstra, A. A.; Lagadec, E.; McDonald, I.; Jones, O.; McGuire, C.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England.
[Oliveira, J. M.; van Loon, J. Th.] Univ Keele, Sch Phys & Geog Sci, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Sargent, B. A.; Volk, K.; Meixner, M.; Sewilo, M.; Shiao, B.; Boyer, M. L.; Gordon, Karl D.; Lawton, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Matsuura, M.] Univ London Univ Coll, Dept Phys & Astron, Inst Origins, London WC1E 6BT, England.
[Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, Inst Origins, Dorking RH5 6NT, Surrey, England.
[Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland.
[Sloan, G. C.; Wilkins, A. N.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Lagadec, E.] European So Observ, D-85748 Garching, Germany.
[Gorjian, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kraemer, K. E.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA.
[Gielen, C.; van Aarle, E.; Van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium.
[Blum, R. D.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Riebel, D.; Srinivasan, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Chen, C. -H. R.; Indebetouw, R.; Leisenring, J. M.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Antoniou, V.; Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Bernard, J. -P.; Olsen, K.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Cohen, M.; Sandstrom, K.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Galametz, M.; Galliano, F.; Harris, J.; Hony, S.; Madden, S.; Rubin, D.] Univ Paris Diderot DAPNIA, CNRS, CEA DSM, Lab AIM, F-91191 Gif Sur Yvette, France.
[Galametz, M.; Galliano, F.; Harris, J.; Hony, S.; Madden, S.; Rubin, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Hora, J. L.; Marengo, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kawamura, A.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 46401, Japan.
[Mulia, A. J.; Speck, A. K.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[O'Halloran, B.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Paladini, R.; Paradis, D.; Reach, W. T.; Van Dyk, S. D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Sandstrom, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Soszynski, I.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Srinivasan, S.] Inst Astrophys, F-75014 Paris, France.
[Tielens, A. G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Vijh, Uma P.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA.
[Whitney, B.] Space Sci Inst, Boulder, CO 80301 USA.
RP Woods, PM (reprint author), Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England.
EM woods@manchester.ac.uk
RI Woods, Paul/E-6926-2011; Van Winckel, Hans/I-7863-2013; Kemper,
Francisca/D-8688-2011; Antoniou, Vallia/E-3837-2013;
OI Reach, William/0000-0001-8362-4094; Woods, Paul/0000-0003-4340-3590; Van
Winckel, Hans/0000-0001-5158-9327; Kemper,
Francisca/0000-0003-2743-8240; Antoniou, Vallia/0000-0001-7539-1593;
Hora, Joseph/0000-0002-5599-4650; Jones, Olivia/0000-0003-4870-5547;
Kraemer, Kathleen/0000-0002-2626-7155; Van Dyk,
Schuyler/0000-0001-9038-9950
FU US Department of Energy through the University of California, Lawrence
Livermore National Laboratory [W-7405-Eng-48]; National Science
Foundation through the Center for Particle Astrophysics of the
University of California [AST-8809616]; Mount Stromlo and Siding Spring
Observatory, Australian National University; National Aeronautics and
Space Administration; National Science Foundation; [N203 511838
(MNiSW)]
FX RSz acknowledges support from grant N203 511838 (MNiSW). This paper
utilizes public domain data obtained by the MACHO project, jointly
funded by the US Department of Energy through the University of
California, Lawrence Livermore National Laboratory under contract no.
W-7405-Eng-48, by the National Science Foundation through the Center for
Particle Astrophysics of the University of California under cooperative
agreement AST-8809616, and by the Mount Stromlo and Siding Spring
Observatory, part of the Australian National University. 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 Optical Gravitational Lensing Experiment OGLE-III
online catalogue of variable stars. This research has made use of the
VizieR catalogue access tool, CDS, Strasbourg, France. This research has
made use of the SIMBAD data base, operated at CDS, Strasbourg, France.
This research has made use of NASA's Astrophysics Data System
Bibliographic Services.
NR 213
TC 55
Z9 55
U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2011
VL 411
IS 3
BP 1597
EP 1627
DI 10.1111/j.1365-2966.2010.17794.x
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 723DL
UT WOS:000287486400016
ER
PT J
AU Yu, JY
Kao, HY
Lee, T
Kim, ST
AF Yu, Jin-Yi
Kao, Hsun-Ying
Lee, Tong
Kim, Seon Tae
TI Subsurface ocean temperature indices for Central-Pacific and
Eastern-Pacific types of El Nio and La Nia events
SO THEORETICAL AND APPLIED CLIMATOLOGY
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; ENSO; NINO
AB Subsurface ocean temperature indices are developed to identify two distinct types of tropical Pacific warming (El Nio) and cooling (La Nia) events: the Eastern-Pacific (EP) type and the Central-Pacific (CP) type. Ocean temperature anomalies in the upper 100 m are averaged over the eastern (80A degrees W-90A degrees W, 5A degrees S-5A degrees N) and central (160A degrees E-150A degrees W, 5A degrees S-5A degrees N) equatorial Pacific to construct the EP and CP subsurface indices, respectively. The analysis is performed for the period of 1958-2001 using an ocean data assimilation product. It is found that the EP/CP subsurface indices are less correlated and show stronger skewness than the sea surface temperature (SST)-based indices. In addition, while both quasi-biennial (similar to 2 years) and quasi-quadrennial (similar to 4 years) periodicities appear in the SST-based indices for these two types, the subsurface indices are dominated only by the quasi-biennial periodicity for the CP type and by the quasi-quadrennial (similar to 4 years) periodicity for the EP type. Low correlation, high skewness, and single leading periodicity are desirable properties for defining indices to separate the EP and CP types. Using the subsurface indices, major El Nio and La Nia events identified by the Nio-3.4 SST index are classified as the EP or CP types for the analysis period. It is found that most strong El Nio events are of the EP type while most strong La Nia events are of the CP type. It is also found that strong CP-type La Nia events tend to occur after strong EP-type El Nio events. The reversed subsequence (i.e., strong EP El Nio events follow strong CP La Nia events) does not appear to be typical. This study shows that subsurface ocean indices are an effective way to identify the EP and CP types of Pacific El Nio and La Nia events.
C1 [Yu, Jin-Yi; 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 NSF [ATM-0925396]; NASA [NNX06AF49H]; JPL [1290687]
FX We thank three anonymous reviewers for their helpful comments. The
research was supported by the NSF (ATM-0925396), NASA (NNX06AF49H), and
JPL (subcontract No. 1290687).
NR 14
TC 42
Z9 51
U1 2
U2 10
PU SPRINGER WIEN
PI WIEN
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA
SN 0177-798X
EI 1434-4483
J9 THEOR APPL CLIMATOL
JI Theor. Appl. Climatol.
PD MAR
PY 2011
VL 103
IS 3-4
BP 337
EP 344
DI 10.1007/s00704-010-0307-6
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 723HZ
UT WOS:000287498700005
ER
PT J
AU Johnson, L
Whorton, M
Heaton, A
Pinson, R
Laue, G
Adams, C
AF Johnson, Les
Whorton, Mark
Heaton, Andy
Pinson, Robin
Laue, Greg
Adams, Charles
TI NanoSail-D: A solar sail demonstration mission
SO ACTA ASTRONAUTICA
LA English
DT Article; Proceedings Paper
CT 6th IAA Symposium on Missions to the Outer Solar System and Beyond
CY JUL 06-09, 2009
CL Aosta, ITALY
SP IAA
DE Solar sail; NanoSail-D; Cubesat
AB In the early to mid-2000s, NASA made substantial progress in the development of solar sail propulsion systems. Solar sail propulsion uses the solar radiation pressure exerted by the momentum transfer of reflected photons to generate a net force on a spacecraft. To date, solar sail propulsion systems were designed for large robotic spacecraft. Recently, however, NASA has been investigating the application of solar sails for small satellite propulsion. The NanoSail-D is a subscale solar sail system designed for possible small spacecraft applications. The NanoSail-D mission flew on board the ill-fated Falcon Rocket launched August 2, 2008, and due to the failure of that rocket, never achieved orbit. The NanoSail-D flight spare is ready for flight and a suitable launch arrangement is being actively pursued. This paper will present an introduction solar sail propulsion systems and an overview of the NanoSail-D spacecraft. Published by Elsevier Ltd.
C1 [Johnson, Les; Whorton, Mark; Heaton, Andy; Pinson, Robin] NASA, George C Marshall Space Flight Ctr, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Laue, Greg] ManTech SRS Technol, Huntsville, AL 35806 USA.
[Adams, Charles] Gray Res Inc, Huntsville, AL 35806 USA.
RP Johnson, L (reprint author), NASA, George C Marshall Space Flight Ctr, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM c.les.johnson@nasa.gov
NR 3
TC 51
Z9 56
U1 6
U2 18
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 MAR-APR
PY 2011
VL 68
IS 5-6
SI SI
BP 571
EP 575
DI 10.1016/j.actaastro.2010.02.008
PG 5
WC Engineering, Aerospace
SC Engineering
GA 717RH
UT WOS:000287064600004
ER
PT J
AU Crabbe, A
Sarker, SF
Van Houdt, R
Ott, CM
Leys, N
Cornelis, P
Nickerson, CA
AF Crabbe, Aurelie
Sarker, Shameema F.
Van Houdt, Rob
Ott, C. Mark
Leys, Natalie
Cornelis, Pierre
Nickerson, Cheryl A.
TI Alveolar epithelium protects macrophages from quorum sensing-induced
cytotoxicity in a three-dimensional co-culture model
SO CELLULAR MICROBIOLOGY
LA English
DT Article
ID HOST-PATHOGEN INTERACTIONS; ROTATING WALL VESSEL; TISSUE-CULTURE MODEL;
ORGANOTYPIC MODELS; INFECTIOUS-DISEASE; ESCHERICHIA-COLI;
CYSTIC-FIBROSIS; CELL-CULTURE; U937 CELLS; IN-VITRO
AB P>The quorum sensing signal N-(3-oxododecanoyl)-l-homoserine lactone (3-oxo-C-12 HSL), produced by Pseudomonas aeruginosa, exerts cytotoxic effects in macrophages in vitro, which is believed to affect host innate immunity in vivo. However, the medical significance of this finding to pulmonary disease remains unclear since the multicellular complexity of the lung was not considered in the assessment of macrophage responses to 3-oxo-C-12 HSL. We developed a novel three-dimensional co-culture model of alveolar epithelium and macrophages using the rotating wall vessel (RWV) bioreactor, by adding undifferentiated monocytes to RWV-derived alveolar epithelium. Our three-dimensional model expressed important architectural/phenotypic hallmarks of the parental tissue, as evidenced by highly differentiated epithelium, spontaneous differentiation of monocytes to functional macrophage-like cells, localization of these cells on the alveolar surface and a macrophage-to-epithelial cell ratio relevant to the in vivo situation. Co-cultivation of macrophages with alveolar epithelium counteracted 3-oxo-C-12 HSL-induced cytotoxicity via removal of quorum sensing molecules by alveolar cells. Furthermore, 3-oxo-C-12 HSL induced the intercellular adhesion molecule ICAM-1 in both alveolar epithelium and macrophages. These data stress the importance of multicellular organotypic models to integrate the role of different cell types in overall lung homeostasis and disease development in response to external factors.
C1 [Crabbe, Aurelie; Sarker, Shameema F.; Nickerson, Cheryl A.] Arizona State Univ, Ctr Infect Dis & Vaccinol, Biodesign Inst, Tempe, AZ 85287 USA.
[Crabbe, Aurelie; Cornelis, Pierre] Vrije Univ Brussel, Flanders Inst Biotechnol VIB, Dept Mol & Cellular Interact, Lab Microbial Interact, B-1050 Brussels, Belgium.
[Crabbe, Aurelie; Van Houdt, Rob; Leys, Natalie] Belgian Nucl Res Ctr SCK CEN, Inst Environm Hlth & Safety, Expert Grp Mol & Cellular Biol, Microbiol Unit, B-2400 Mol, Belgium.
[Ott, C. Mark] NASA, Lyndon B Johnson Space Ctr, Habitabil & Environm Factors Off, Houston, TX 77058 USA.
RP Crabbe, A (reprint author), Arizona State Univ, Ctr Infect Dis & Vaccinol, Biodesign Inst, 1001 S McAllister Ave, Tempe, AZ 85287 USA.
EM acrabbe@asu.edu
RI Van Houdt, Rob/B-8599-2011
OI Van Houdt, Rob/0000-0002-7459-496X
FU Belgian American Educational Foundation (BAEF); King Baudouin
Foundation; European Space Agency (ESA); Belgian Science Policy
(Belspo); NASA [NCC2-1362, NNJ04HF75F, NNJ06HE92]; NIH [R21MH080702]
FX The authors are grateful to Doug Daniel for assistance with CLSM
imaging, performed at the Center for BioOptical Nanotechnology in the
Biodesign Institute (ASU); and Melissa Herbst-Kralovetz (ASU) for
helpful discussions. We express our gratitude to Myriam Ghardi (SCK.CEN)
and Mike Hansen (ASU) for helpful advice regarding flow cytometry
experiments; Roy Curtiss III (ASU) and Sarah Baatout (SCK.CEN) for their
generosity in allowing us to use their respective flow cytometry
devices. Aurelie Crabbe was financially supported by a Henri Benedictus
Fellowship from the Belgian American Educational Foundation (BAEF) and
the King Baudouin Foundation, and a research grant of the European Space
Agency (ESA) and the Belgian Science Policy (Belspo). This research was
funded in the lab of Cheryl Nickerson (ASU) by NASA Grants NCC2-1362,
NNJ04HF75F, NNJ06HE92; and NIH Grant R21MH080702.
NR 60
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Z9 11
U1 1
U2 20
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1462-5814
J9 CELL MICROBIOL
JI Cell Microbiol.
PD MAR
PY 2011
VL 13
IS 3
BP 469
EP +
DI 10.1111/j.1462-5822.2010.01548.x
PG 13
WC Cell Biology; Microbiology
SC Cell Biology; Microbiology
GA 720XX
UT WOS:000287317100001
PM 21054742
ER
PT J
AU Thomassen, HA
Fuller, T
Buermann, W
Mila, B
Kieswetter, CM
Jarrin, P
Cameron, SE
Mason, E
Schweizer, R
Schlunegger, J
Chan, J
Wang, O
Peralvo, M
Schneider, CJ
Graham, CH
Pollinger, JP
Saatchi, S
Wayne, RK
Smith, TB
AF Thomassen, Henri A.
Fuller, Trevon
Buermann, Wolfgang
Mila, Borja
Kieswetter, Charles M.
Jarrin-, Pablo, V
Cameron, Susan E.
Mason, Eliza
Schweizer, Rena
Schlunegger, Jasmin
Chan, Janice
Wang, Ophelia
Peralvo, Manuel
Schneider, Christopher J.
Graham, Catherine H.
Pollinger, John P.
Saatchi, Sassan
Wayne, Robert K.
Smith, Thomas B.
TI Mapping evolutionary process: a multi-taxa approach to conservation
prioritization
SO EVOLUTIONARY APPLICATIONS
LA English
DT Article
DE Andes; conservation prioritization; ecological modeling; Ecuador;
evolutionary process; generalized dissimilarity modeling; landscape
genetics; species distribution
ID CLIMATE-CHANGE; BIODIVERSITY HOTSPOTS; PLACE PRIORITIZATION;
SOUTH-AMERICA; MODIS DATA; DIVERSITY; SELECTION; ECUADOR; AREAS;
DISTRIBUTIONS
AB Human-induced land use changes are causing extensive habitat fragmentation. As a result, many species are not able to shift their ranges in response to climate change and will likely need to adapt in situ to changing climate conditions. Consequently, a prudent strategy to maintain the ability of populations to adapt is to focus conservation efforts on areas where levels of intraspecific variation are high. By doing so, the potential for an evolutionary response to environmental change is maximized. Here, we use modeling approaches in conjunction with environmental variables to model species distributions and patterns of genetic and morphological variation in seven Ecuadorian amphibian, bird, and mammal species. We then used reserve selection software to prioritize areas for conservation based on intraspecific variation or species-level diversity. Reserves selected using species richness and complementarity showed little overlap with those based on genetic and morphological variation. Priority areas for intraspecific variation were mainly located along the slopes of the Andes and were largely concordant among species, but were not well represented in existing reserves. Our results imply that in order to maximize representation of intraspecific variation in reserves, genetic and morphological variation should be included in conservation prioritization.
C1 [Thomassen, Henri A.; Fuller, Trevon; Buermann, Wolfgang; Mila, Borja; Chan, Janice; Pollinger, John P.; Saatchi, Sassan; Wayne, Robert K.; Smith, Thomas B.] Univ Calif Los Angeles, Inst Environm, Ctr Trop Res, Los Angeles, CA 90095 USA.
[Buermann, Wolfgang] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Mila, Borja] Consejo Super Invest Cient, Museo Nacl Ciencias Nat, Madrid, Spain.
[Kieswetter, Charles M.; Schneider, Christopher J.] Boston Univ, Dept Biol, Boston, MA 02215 USA.
[Jarrin-, Pablo, V] Pontificia Univ Catolica Ecuador, Yasuni Res Stn, Escuela Ciencias Biol, Quito, Ecuador.
[Cameron, Susan E.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA.
[Cameron, Susan E.] Harvard Univ, Ctr Environm, Cambridge, MA 02138 USA.
[Mason, Eliza; Schweizer, Rena; Schlunegger, Jasmin; Pollinger, John P.; Wayne, Robert K.; Smith, Thomas B.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Mason, Eliza] Univ N Carolina, Sch Med, Chapel Hill, NC USA.
[Wang, Ophelia] Univ Texas Austin, Dept Geog & Environm, Austin, TX 78712 USA.
[Peralvo, Manuel] CONDESAN, Unidad Biodiversidad & Geog Aplicada, Quito, Ecuador.
[Graham, Catherine H.] SUNY Stony Brook, Dept Ecol & Evolut, New York, NY USA.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Thomassen, HA (reprint author), Univ Calif Los Angeles, Inst Environm, Ctr Trop Res, La Kretz Hall,Suite 300,619 Charles E Young Dr E, Los Angeles, CA 90095 USA.
EM hathomassen@ucla.edu
RI Graham, Catherine/A-9560-2011; Cameron Devitt, Susan/E-2659-2013;
OI Mila, Borja/0000-0002-6446-0079
FU NSF [IRCEB9977072]; NASA [IDS/03-0169-0347, NNG05GB37G]
FX For help in the field we thank Fernando Alaya, Diego Almeida-Reinoso,
Italo Tapia, Juan Fernando Freile, Tatiana Santander, Jaime Chaves,
Gabriela Castaneda, Brandt T. Ryder, Daniela Gross, Juan Diego Ortiz,
Orfa Rodriguez, Maria Fernanda Salazar, Suzanne Tomassi, John McCormack,
Brenda Larison, Luis Carrasco, Marcelo Tobar, Jordan Karubian, and the
Timpe family. We also thank Martin R. Bustamante, Santiago R. Ron, and
Juan Manuel Guayasamin for frog specimen identification and locality
data; Elisa Bonaccorso for facilitating molecular laboratory work on the
frogs; Nestor Acosta-Buenano and Pablo Menendez-Guerrero for frog
locality data; Monica Paez and Andrea Teran for assistance in frog
identification; Luis A. Coloma (Museo de Zoologia at Pontifica
Universidad Catolica del Ecuador (PUCE)) for tissue loans; and the
Kansas University of Natural History for access to the collection. We
are grateful to Dr. M. Kinnison and two anonymous reviewers for
thoughtful comments on a previous version of this manuscript. For
assistance on woodcreeper work in the laboratory, we thank Navi Timber
and Daniel Greenfield. Funding was provided by grants from NSF
(IRCEB9977072 to TBS, RKW, and CJS) and NASA (IDS/03-0169-0347 to TBS,
RKW, and CJS; NNG05GB37G to CHG).
NR 78
TC 29
Z9 31
U1 13
U2 91
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1752-4571
J9 EVOL APPL
JI Evol. Appl.
PD MAR
PY 2011
VL 4
IS 2
BP 397
EP 413
DI 10.1111/j.1752-4571.2010.00172.x
PG 17
WC Evolutionary Biology
SC Evolutionary Biology
GA 722RK
UT WOS:000287451800017
PM 25567981
ER
PT J
AU Hornby, GS
Lohn, JD
Linden, DS
AF Hornby, Gregory. S.
Lohn, Jason D.
Linden, Derek S.
TI Computer-Automated Evolution of an X-Band Antenna for NASA's Space
Technology 5 Mission
SO EVOLUTIONARY COMPUTATION
LA English
DT Article
DE Antenna; automated design; computational design; evolutionary design;
generative representation; spacecraft
ID MODULAR PHYSICAL ROBOTS; GENETIC ALGORITHMS; DESIGN
AB Whereas the current practice of designing antennas by hand is severely limited because it is both time and labor intensive and requires a significant amount of domain knowledge, evolutionary algorithms can be used to search the design space and automatically find novel antenna designs that are more effective than would otherwise be developed. Here we present our work in using evolutionary algorithms to automatically design an X-band antenna for NASA's Space Technology 5 (ST5) spacecraft. Two evolutionary algorithms were used: the first uses a vector of real-valued parameters and the second uses a tree-structured generative representation for constructing the antenna. The highest-performance antennas from both algorithms were fabricated and tested and both outperformed a hand-designed antenna produced by the antenna contractor for the mission. Subsequent changes to the spacecraft orbit resulted in a change in requirements for the spacecraft antenna. By adjusting our fitness function we were able to rapidly evolve a new set of antennas for this mission in less than a month. One of these new antenna designs was built, tested, and approved for deployment on the three ST5 spacecraft, which were successfully launched into space on March 22, 2006. This evolved antenna design is the first computer-evolved antenna to be deployed for any application and is the first computer-evolved hardware in space.
C1 [Hornby, Gregory. S.] UC Santa Cruz, Univ Affiliated Res Ctr, Moffett Field, CA 94035 USA.
[Lohn, Jason D.] Carnegie Mellon Univ, Moffett Field, CA 94035 USA.
[Linden, Derek S.] X5 Syst Inc, Ashburn, VA 20147 USA.
RP Hornby, GS (reprint author), UC Santa Cruz, Univ Affiliated Res Ctr, NASA Ames Res Pk, Moffett Field, CA 94035 USA.
EM Gregory.S.Hornby@nasa.gov; Jason.Lohn@sv.cmu.edu; dlinden@x5systems.com
FU Mission and Science Measurement Technology, NASA Headquarters
FX The work described in this paper was supported by Mission and Science
Measurement Technology, NASA Headquarters, under its Computing,
Information, and Communications Technology Program. The work was
performed at the Intelligent Systems Division, NASA Ames Research
Center, Linden Innovation Research, and NASA Goddard Space Flight
Center. We gratefully acknowledge the support of Ken Perko of Microwave
Systems Branch at NASA Goddard and Bruce Blevins of the Physical Science
Laboratory at New Mexico State University.
NR 25
TC 28
Z9 28
U1 1
U2 4
PU MIT PRESS
PI CAMBRIDGE
PA 55 HAYWARD STREET, CAMBRIDGE, MA 02142 USA
SN 1063-6560
J9 EVOL COMPUT
JI Evol. Comput.
PD SPR
PY 2011
VL 19
IS 1
BP 1
EP 23
DI 10.1162/EVCO_a_00005
PG 23
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA 720IG
UT WOS:000287273700001
PM 20583909
ER
PT J
AU Wang, WL
Dungan, J
Hashimoto, H
Michaelis, AR
Milesi, C
Ichii, K
Nemani, RR
AF Wang, Weile
Dungan, Jennifer
Hashimoto, Hirofumi
Michaelis, Andrew R.
Milesi, Cristina
Ichii, Kazuhito
Nemani, Ramakrishna R.
TI Diagnosing and assessing uncertainties of terrestrial ecosystem models
in a multimodel ensemble experiment: 1. Primary production
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE biogeochemistry; carbon cycle; model intercomparison; model uncertainty;
multimodel ensemble; primary production; terrestrial ecosystem model
ID NET PRIMARY PRODUCTIVITY; GROSS PRIMARY PRODUCTION; CARBON-DIOXIDE
EXCHANGE; COMPARING GLOBAL-MODELS; LEAF-AREA INDEX; ATMOSPHERIC CO2;
CONSTANT FRACTION; SATELLITE DATA; CLIMATE; MODIS
AB We conducted an ensemble modeling exercise using the Terrestrial Observation and Prediction System (TOPS) to evaluate sources of uncertainty in carbon flux estimates resulting from structural differences among ecosystem models. The experiment ran public-domain versions of biome-bgc, lpj, casa, and tops-bgc over North America at 8 km resolution and for the period of 1982-2006. We developed the Hierarchical Framework for Diagnosing Ecosystem Models (HFDEM) to separate the simulated biogeochemistry into a cascade of three functional tiers and sequentially examine their characteristics in climate (temperature-precipitation) and other spaces. Analysis of the simulated annual gross primary production (GPP) in the climate domain indicates a general agreement among the models, all showing optimal GPP in regions where the relationship between annual average temperature (T, degrees C) and annual total precipitation (P, mm) is defined by P=50T+500. However, differences in simulated GPP are identified in magnitudes and distribution patterns. For forests, the GPP gradient along P=50T+500 ranges from similar to 50 g C yr-1 m-2 degrees C-1 (casa) to similar to 125 g C yr-1 m-2 degrees C-1 (biome-bgc) in cold/temperate regions; for nonforests, the diversity among GPP distributions is even larger. Positive linear relationships are found between annual GPP and annual mean leaf area index (LAI) in all models. For biome-bgc and lpj, such relationships lead to a positive feedback from LAI growth to GPP enhancement. Different approaches to constrain this feedback lead to different sensitivity of the models to disturbances such as fire, which contribute significantly to the diversity in GPP stated above. The ratios between independently simulated NPP and GPP are close to 50% on average; however, their distribution patterns vary significantly between models, reflecting the difficulties in estimating autotrophic respiration across various climate regimes. Although these results are drawn from our experiments with the tested model versions, the developed methodology has potential for other model exercises.
C1 [Wang, Weile; Dungan, Jennifer; Hashimoto, Hirofumi; Michaelis, Andrew R.; Milesi, Cristina; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wang, Weile; Hashimoto, Hirofumi; Michaelis, Andrew R.; Milesi, Cristina] Calif State Univ, Seaside, CA USA.
[Ichii, Kazuhito] Fukushima Univ, Fac Symbiot Syst Sci, Fukushima, Japan.
RP Nemani, RR (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM weile.wang@gmail.com
RI Ichii, Kazuhito/D-2392-2010; Dungan, Jennifer/G-9921-2016
OI Ichii, Kazuhito/0000-0002-8696-8084; Dungan,
Jennifer/0000-0002-4863-1616
FU National Science Foundation (NSF); NASA
FX The dataset GSOD is from NOAA NCDC (http://www.ncdc.noaa.gov). The
dataset TD3200 is from the Research Data Archive (RDA), which is
maintained by the Computational and Information Systems Laboratory
(CISL) at the National Center for Atmospheric Research (NCAR). NCAR is
sponsored by the National Science Foundation (NSF). The original data
are available from the RDA (http://dss.ucar.edu) in dataset number
ds510.0. This research was funded by grants from the NASA Earth Science
program. The authors thank two anonymous reviewers for their insightful
comments and constructive suggestions.
NR 60
TC 32
Z9 32
U1 3
U2 50
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD MAR
PY 2011
VL 17
IS 3
BP 1350
EP 1366
DI 10.1111/j.1365-2486.2010.02309.x
PG 17
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 714VU
UT WOS:000286837900009
ER
PT J
AU Wang, WL
Dungan, J
Hashimoto, H
Michaelis, AR
Milesi, C
Ichii, K
Nemani, RR
AF Wang, Weile
Dungan, Jennifer
Hashimoto, Hirofumi
Michaelis, Andrew R.
Milesi, Cristina
Ichii, Kazuhito
Nemani, Ramakrishna R.
TI Diagnosing and assessing uncertainties of terrestrial ecosystem models
in a multimodel ensemble experiment: 2. Carbon balance
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE biogeochemistry; carbon balance; carbon cycle; model intercomparison;
model uncertainty; multimodel ensemble; terrestrial ecosystem model
ID GLOBAL VEGETATION MODELS; PRIMARY PRODUCTIVITY NPP; LEAF-AREA INDEX;
PLANT GEOGRAPHY; CLIMATE; DYNAMICS; SYSTEM; DISTURBANCE; SURFACES;
FUTURE
AB This paper examines carbon stocks and their relative balance in terrestrial ecosystems simulated by Biome-BGC, LPJ, and CASA in an ensemble model experiment conducted using the Terrestrial Observation and Prediction System. We developed the Hierarchical Framework for Diagnosing Ecosystem Models to separate the simulated biogeochemistry into a cascade of functional tiers and examine their characteristics sequentially. The analyses indicate that the simulated biomass is usually two to three times higher in Biome-BGC than LPJ or CASA. Such a discrepancy is mainly induced by differences in model parameters and algorithms that regulate the rates of biomass turnover. The mean residence time of biomass in Biome-BGC is estimated to be 40-80 years in temperate/moist climate regions, while it mostly varies between 5 and 30 years in CASA and LPJ. A large range of values is also found in the simulated soil carbon. The mean residence time of soil carbon in Biome-BGC and LPJ is similar to 200 years in cold regions, which decreases rapidly with increases of temperature at a rate of similar to 10 yr degrees C-1. Because long-term soil carbon pool is not simulated in CASA, its corresponding mean residence time is only about 10-20 years and less sensitive to temperature. Another key factor that influences the carbon balance of the simulated ecosystem is disturbance caused by wildfire, for which the algorithms vary among the models. Because fire emissions are balanced by net ecosystem production (NEP) at steady states, magnitudes, and spatial patterns of NEP vary significantly as well. Slight carbon imbalance may be left by the spin-up algorithm of the models, which adds uncertainty to the estimated carbon sources or sinks. Although these results are only drawn on the tested model versions, the developed methodology has potential for other model exercises.
C1 [Wang, Weile; Dungan, Jennifer; Hashimoto, Hirofumi; Michaelis, Andrew R.; Milesi, Cristina; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wang, Weile; Hashimoto, Hirofumi; Michaelis, Andrew R.; Milesi, Cristina] Calif State Univ, Seaside, CA 93955 USA.
[Ichii, Kazuhito] Fukushima Univ, Fac Symbiot Syst Sci, Fukushima 9601296, Japan.
RP Wang, WL (reprint author), NASA, Ames Res Ctr, Mail Stop 242-4, Moffett Field, CA 94035 USA.
EM weile.wang@gmail.com
RI Ichii, Kazuhito/D-2392-2010; Dungan, Jennifer/G-9921-2016
OI Ichii, Kazuhito/0000-0002-8696-8084; Dungan,
Jennifer/0000-0002-4863-1616
FU National Science Foundation (NSF); NASA
FX The dataset GSOD is from NOAA NCDC (http://www.ncdc.noaa.gov). The
dataset TD3200 is from the Research Data Archive (RDA), which is
maintained by the Computational and Information Systems Laboratory
(CISL) at the National Center for Atmospheric Research (NCAR). NCAR is
sponsored by the National Science Foundation (NSF). The original data
are available from the RDA (http://dss.ucar.edu) in dataset number
ds510.0. This research was funded by grants from the NASA Earth Science
program. We thank two anonymous reviewers for their insightful comments.
NR 29
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U1 0
U2 32
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD MAR
PY 2011
VL 17
IS 3
BP 1367
EP 1378
DI 10.1111/j.1365-2486.2010.02315.x
PG 12
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 714VU
UT WOS:000286837900010
ER
PT J
AU Czarnek, R
Skrzat, A
Lin, SY
AF Czarnek, R.
Skrzat, A.
Lin, S. Y.
TI Application of Moire interferometry to reconstruction of residual stress
in cut railroad car wheels
SO MEASUREMENT
LA English
DT Article
DE Moire interferometry; Residual stress; Railroad wheel
AB Railroad car wheels develop residual stresses both in their manufacture and while in service. Knowledge of the residual stress distribution and its variation over time is necessary for the prediction of wheel service life and possible catastrophic failure. It is also vital for the safety of railway transportation. Although a theoretical solution is possible, it remains complex. Alternatively, the solution may be also obtained by using experimental measurements assisted by the theory of mechanics. An approach known as "physically-based enhancement of experimental data" formulated and subsequently developed and tested is the best available experimental-numerical tool for the reconstruction of acquired residual hoop stress component in railroad car wheels. This paper presents the formulation, approach and results of the analysis performed on experimental data obtained from investigations of the passenger and freight wheels during a saw cutting process. A discussion on the precision of the results has been included. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Czarnek, R.] Czarnek & Orkin Labs Inc, Johnstown, PA USA.
[Skrzat, A.] Rzeszow Univ Technol, Dept Mat Forming & Proc, Rzeszow, Poland.
[Lin, S. Y.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Czarnek, R (reprint author), Czarnek & Orkin Labs Inc, Johnstown, PA USA.
EM czarnek@atlanticbb.net; askrzat@prz.rzeszow.pl; shih-yung.lin@nasa.gov
NR 14
TC 2
Z9 2
U1 0
U2 0
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0263-2241
J9 MEASUREMENT
JI Measurement
PD MAR
PY 2011
VL 44
IS 3
BP 569
EP 579
DI 10.1016/j.measurement.2010.11.019
PG 11
WC Engineering, Multidisciplinary; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 720IV
UT WOS:000287275200009
ER
PT J
AU Liu, J
Basu, S
Lutz, RR
AF Liu, Jing
Basu, Samik
Lutz, Robyn R.
TI Compositional model checking of software product lines using variation
point obligations
SO AUTOMATED SOFTWARE ENGINEERING
LA English
DT Article
DE Software product lines; Compositional model checking; Variation point;
Feature
ID SPECIFICATIONS; VERIFICATION; SYSTEMS
AB This paper introduces a technique for incremental and compositional model checking that allows efficient reuse of model-checking results associated with the features in a product line. As the use of product lines has increased, so has the need to verify the models used to construct the products in the product line. However, this effort is currently hampered by the difficulty of composing model-checking results for the features in a way that allows reuse for subsequent products. The contributions of this paper are to remove restrictions on how the features can be sequentially composed, to describe how to generate obligations such that all sequentially composed systems can be verified, and to show how to compositionally model check the product in the product line by reusing the variation-point obligations. The paper develops the technique and its implementation in the context of a medical-device product line.
C1 [Liu, Jing] Rockwell Collins Inc, Cedar Rapids, IA 52498 USA.
[Basu, Samik; Lutz, Robyn R.] Iowa State Univ, Dept Comp Sci, Ames, IA USA.
[Lutz, Robyn R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Liu, J (reprint author), Rockwell Collins Inc, Cedar Rapids, IA 52498 USA.
EM Jing.Janet.Liu@gmail.com; sbasu@cs.iastate.edu; rlutz@cs.iastate.edu
FU National Science Foundation [0541163, 0702758, 0709217, 0916275]
FX This research was supported by the National Science Foundation under
grants 0541163, 0702758, 0709217 and 0916275. The authors would like to
thank members of the IFIP Working Group 2.9, Software Requirements
Engineering, for valuable feedback on a presentation describing this
work.
NR 49
TC 14
Z9 14
U1 0
U2 3
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0928-8910
J9 AUTOMAT SOFTW ENG
JI Automat. Softw. Eng.
PD MAR
PY 2011
VL 18
IS 1
BP 39
EP 76
DI 10.1007/s10515-010-0075-7
PG 38
WC Computer Science, Software Engineering
SC Computer Science
GA 702CV
UT WOS:000285873100003
ER
PT J
AU Randall, JP
Meador, MAB
Jana, SC
AF Randall, Jason P.
Meador, Mary Ann B.
Jana, Sadhan C.
TI Tailoring Mechanical Properties of Aerogels for Aerospace Applications
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE silica aerogel; polymer cross-linking; nanoporous materials; flexible
aerogels; sol-gel; conformal coatings; skeletal density
ID ORGANIC-INORGANIC MATERIALS; LINKED SILICA AEROGELS; AMINE-MODIFIED
SILICA; COHERENT EXPANDED AEROGELS; POROUS 3D NANOSTRUCTURES; BRIDGED
POLYSILSESQUIOXANES; THERMAL-CONDUCTIVITY; ACOUSTIC PROPERTIES; ELASTIC
PROPERTIES; ALUMINA AEROGELS
AB Silica aerogels are highly porous solid materials consisting of three-dimensional networks of silica particles and are typically obtained by removing the liquid in silica gels under supercritical conditions. Several unique attributes such as;extremely low thermal conductivity and low density make silica aerogels excellent candidates in the quest for thermal insulation materials used in space missions. However, native silica aerogels are fragile at relatively low stresses. M:ore durable aerogels with higher strength and stiffness are obtained by proper selection of silane precursors and by reinforcement with polymers. This paper first presents a brief review of the literature on methods of silica aerogel reinforcement and then discusses our recent activities in improving not only the strength but also the elastic response of polymer-reinforced silica aerogels. Several alkyl-linked bis-silanes were used in promoting flexibility of the silica networks in conjunction with polymer reinforcement by epoxy.
C1 [Meador, Mary Ann B.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Randall, Jason P.; Jana, Sadhan C.] Univ Akron, Dept Polymer Engn, Akron, OH 44325 USA.
RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM maryann.meador@nasa.gov; janas@uakron.edu
RI Jana, Sadhan/J-5467-2016;
OI Jana, Sadhan/0000-0001-8962-380X; Meador, Mary Ann/0000-0003-2513-7372
FU Fundamental Aeronautics Program (Subsonics Rotary Wing and Hypersonics);
NASA
FX We thank the Fundamental Aeronautics Program (Subsonics Rotary Wing and
Hypersonics) and the NASA Graduate Student Researcher Program for
funding this work. We also thank Ms. Linda McCorkle for providing SEM
analysis, Mr. Dan Schieman for thermal analysis and helium pycnometry
measurements, and Ms. Anna Palczer and Dr. Baochau Nguyen for nitrogen
porosimetry results.
NR 91
TC 130
Z9 133
U1 21
U2 204
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD MAR
PY 2011
VL 3
IS 3
BP 613
EP 626
DI 10.1021/am200007n
PG 14
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA 739AV
UT WOS:000288685200001
PM 21361281
ER
PT J
AU Haan, S
Surace, JA
Armus, L
Evans, AS
Howell, JH
Mazzarella, JM
Kim, DC
Vavilkin, T
Inami, H
Sanders, DB
Petric, A
Bridge, CR
Melbourne, JL
Charmandaris, V
Diaz-Santos, T
Murphy, EJ
U, V
Stierwalt, S
Marshall, JA
AF Haan, S.
Surace, J. A.
Armus, L.
Evans, A. S.
Howell, J. H.
Mazzarella, J. M.
Kim, D. C.
Vavilkin, T.
Inami, H.
Sanders, D. B.
Petric, A.
Bridge, C. R.
Melbourne, J. L.
Charmandaris, V.
Diaz-Santos, T.
Murphy, E. J.
U, V.
Stierwalt, S.
Marshall, J. A.
TI THE NUCLEAR STRUCTURE IN NEARBY LUMINOUS INFRARED GALAXIES: HUBBLE SPACE
TELESCOPE NICMOS IMAGING OF THE GOALS SAMPLE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: bulges; galaxies: evolution; galaxies:
interactions; galaxies: starburst; infrared: galaxies
ID ULTRALUMINOUS IRAS GALAXIES; STAR-FORMATION HISTORY; BLACK-HOLE MASS;
SKY LIRG SURVEY; ELLIPTIC GALAXIES; MERGER REMNANTS; EXTRA LIGHT;
INTERACTING GALAXIES; BRIGHTNESS PROFILES; BURIED STARBURST
AB We present results of Hubble Space Telescope (HST) NICMOS H-band imaging of 73 of the most luminous (i.e., log[L-IR/L-circle dot] > 11.4) infrared galaxies (LIRGs) in the Great Observatories All-sky LIRG Survey. This data set combines multi-wavelength imaging and spectroscopic data from space-based (Spitzer, HST, GALEX, and Chandra) and ground-based telescopes. In this paper, we use high-resolution near-infrared data to recover nuclear structure that is obscured by dust at optical wavelengths and measure the evolution in this structure along the merger sequence. A large fraction of all galaxies in our sample possess double nuclei (similar to 63%) or show evidence for triple nuclei (similar to 6%). Half of these double nuclei are not visible in the HST B-band images due to dust obscuration. The majority of interacting LIRGs have remaining merger timescales of 0.3-1.3 Gyr, based on the projected nuclear separations and the mass ratio of nuclei. We find that the bulge luminosity surface density L-Bulge/R-Bulge(2) increases significantly along the merger sequence (primarily due to a decrease of the bulge radius), while the bulge luminosity shows a small increase toward late merger stages. No significant increase of the bulge Sersic index is found. LIRGs that show no interaction features have on average a significantly larger bulge luminosity, suggesting that non-merging LIRGs have larger bulge masses than merging LIRGs. This may be related to the flux-limited nature of the sample and the fact that mergers can significantly boost the IR luminosity of otherwise low luminosity galaxies. We find that the projected nuclear separation is significantly smaller for ULIRGs (median value of 1.2 kpc) than for LIRGs (median value of 6.7 kpc), suggesting that the LIRG phase appears earlier in mergers than the ULIRG phase.
C1 [Haan, S.; Surace, J. A.; Armus, L.; Howell, J. H.; Inami, H.; Petric, A.; Murphy, E. J.; Stierwalt, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Evans, A. S.; Kim, D. C.; Marshall, J. A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Evans, A. S.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Mazzarella, J. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Inami, H.] Grad Univ Adv Studies, Dept Space & Astronaut Sci, Sokendai, Japan.
[Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Bridge, C. R.; Melbourne, J. L.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
[Bridge, C. R.; Melbourne, J. L.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece.
[Charmandaris, V.] IESL Fdn Res & Technol Hellas, GR-71110 Iraklion, Greece.
[Charmandaris, V.] Observ Paris, F-75014 Paris, France.
[Marshall, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Haan, S (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RI Charmandaris, Vassilis/A-7196-2008; Diaz-Santos, Tanio/B-4875-2011;
OI Charmandaris, Vassilis/0000-0002-2688-1956; Mazzarella,
Joseph/0000-0002-8204-8619
FU National Aeronautics and Space Administration [NAS 5-26555]; NASA from
the Space Telescope Science Institute [HST GO 11235.01-A]
FX The authors wish to thank Philip F. Hopkins for valuable discussions of
our results in terms of model predictions and numerical simulations. We
are also grateful for useful suggestions by the referee, which helped
improve this paper. This research has made use of the NASA/IPAC
Extragalactic Database (NED) and Infrared Science Archive which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. Support for this work was provided through grant HST GO
11235.01-A by NASA 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.
NR 86
TC 51
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2011
VL 141
IS 3
AR 100
DI 10.1088/0004-6256/141/3/100
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 719TC
UT WOS:000287231000031
ER
PT J
AU Harris, AW
Mommert, M
Hora, JL
Mueller, M
Trilling, DE
Bhattacharya, B
Bottke, WF
Chesley, S
Delbo, M
Emery, JP
Fazio, G
Mainzer, A
Penprase, B
Smith, HA
Spahr, TB
Stansberry, JA
Thomas, CA
AF Harris, A. W.
Mommert, M.
Hora, J. L.
Mueller, M.
Trilling, D. E.
Bhattacharya, B.
Bottke, W. F.
Chesley, S.
Delbo, M.
Emery, J. P.
Fazio, G.
Mainzer, A.
Penprase, B.
Smith, H. A.
Spahr, T. B.
Stansberry, J. A.
Thomas, C. A.
TI ExploreNEOs. II. THE ACCURACY OF THE WARM SPITZER NEAR-EARTH OBJECT
SURVEY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; minor planets, asteroids: general; surveys
ID THERMAL INFRARED OBSERVATIONS; SPACE-TELESCOPE; RADIOMETRIC DIAMETER;
ARRAY CAMERA; ASTEROIDS; ALBEDO; SIZE; MISSION; MODEL; EROS
AB We report on results of observations of near-Earth objects (NEOs) performed with the NASA Spitzer Space Telescope as part of our ongoing (2009-2011) Warm Spitzer NEO survey ("ExploreNEOs"), the primary aim of which is to provide sizes and albedos of some 700 NEOs. The emphasis of the work described here is an assessment of the overall accuracy of our survey results, which are based on a semi-empirical generalized model of asteroid thermal emission. The NASA Spitzer Space Telescope has been operated in the so-called Warm Spitzer mission phase since the cryogen was depleted in 2009 May, with the two shortest-wavelength channels, centered at 3.6 mu m and 4.5 mu m, of the Infrared Array Camera continuing to provide valuable data. The set of some 170 NEOs in our current Warm Spitzer results catalog contains 28 for which published taxonomic classifications are available, and 14 for which relatively reliable published diameters and albedos are available. A comparison of the Warm Spitzer results with previously published results ("ground truth"), complemented by a Monte Carlo error analysis, indicates that the rms Warm Spitzer diameter and albedo errors are +/- 20% and +/- 50%, respectively. Cases in which agreement with results from the literature is worse than expected are highlighted and discussed; these include the potential spacecraft target 138911 2001 AE(2). We confirm that 1.4 appears to be an appropriate overall default value for the relative reflectance between the V band and the Warm Spitzer wavelengths, for use in correction of the Warm Spitzer fluxes for reflected solar radiation.
C1 [Harris, A. W.; Mommert, M.] DLR Inst Planetary Res, D-12489 Berlin, Germany.
[Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mueller, M.; Delbo, M.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France.
[Trilling, D. E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA.
[Bhattacharya, B.] NASA Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA.
[Chesley, S.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Penprase, B.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Stansberry, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Harris, AW (reprint author), DLR Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM alan.harris@dlr.de
OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650;
Thomas, Cristina/0000-0003-3091-5757
FU NASA; DFG [SPP 1385]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Liberal
use was made of the excellent JPL Horizons System for generating
ephemerides. We acknowledge support by DFG through SPP 1385: The first
ten million years of the solar system-a planetary materials approach. We
thank the anonymous referee for comments that led to significant
improvements in the paper.
NR 50
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2011
VL 141
IS 3
AR 75
DI 10.1088/0004-6256/141/3/75
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 719TC
UT WOS:000287231000006
ER
PT J
AU Prsa, A
Batalha, N
Slawson, RW
Doyle, LR
Welsh, WF
Orosz, JA
Seager, S
Rucker, M
Mjaseth, K
Engle, SG
Conroy, K
Jenkins, J
Caldwell, D
Koch, D
Borucki, W
AF Prsa, Andrej
Batalha, Natalie
Slawson, Robert W.
Doyle, Laurance R.
Welsh, William F.
Orosz, Jerome A.
Seager, Sara
Rucker, Michael
Mjaseth, Kimberly
Engle, Scott G.
Conroy, Kyle
Jenkins, Jon
Caldwell, Douglas
Koch, David
Borucki, William
TI KEPLER ECLIPSING BINARY STARS. I. CATALOG AND PRINCIPAL CHARACTERIZATION
OF 1879 ECLIPSING BINARIES IN THE FIRST DATA RELEASE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; catalogs; methods: data analysis; methods:
numerical; methods: statistical; stars: fundamental parameters
ID SMALL-MAGELLANIC-CLOUD; GRAVITATIONAL LENSING EXPERIMENT; SKY AUTOMATED
SURVEY; VARIABLE-STARS; INITIAL CHARACTERISTICS; PHOTOMETRIC SOLUTIONS;
DISTANCE INDICATORS; IMAGE SUBTRACTION; STELLAR EVOLUTION; CADENCE DATA
AB The Kepler space mission is devoted to finding Earth-size planets orbiting other stars in their habitable zones. Its large, 105 deg(2) field of view features over 156,000 stars that are observed continuously to detect and characterize planet transits. Yet, this high-precision instrument holds great promise for other types of objects as well. Here we present a comprehensive catalog of eclipsing binary stars observed by Kepler in the first 44 days of operation, the data being publicly available through MAST as of 2010 June 15. The catalog contains 1879 unique objects. For each object, we provide its Kepler ID ( KID), ephemeris (BJD(0), P-0), morphology type, physical parameters (T-eff, log g, E(B - V)), the estimate of third light contamination (crowding), and principal parameters (T-2/T-1, q, fillout factor, and sin i for overcontacts, and T-2/T-1, (R-1 + R-2)/ a, e sin omega, e cos omega, and sin i for detached binaries). We present statistics based on the determined periods and measure the average occurrence rate of eclipsing binaries to be similar to 1.2% across the Kepler field. We further discuss the distribution of binaries as a function of galactic latitude and thoroughly explain the application of artificial intelligence to obtain principal parameters in a matter of seconds for the whole sample. The catalog was envisioned to serve as a bridge between the now public Kepler data and the scientific community interested in eclipsing binary stars.
C1 [Prsa, Andrej; Engle, Scott G.; Conroy, Kyle] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Batalha, Natalie; Rucker, Michael; Mjaseth, Kimberly] San Jose State Univ, San Jose, CA 95192 USA.
[Slawson, Robert W.; Doyle, Laurance R.] SETI Inst, Mountain View, CA 94043 USA.
[Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, San Diego, CA 92182 USA.
[Seager, Sara] MIT, Cambridge, MA 02139 USA.
[Jenkins, Jon; Caldwell, Douglas] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Prsa, A (reprint author), Villanova Univ, Dept Astron & Astrophys, 800 E Lancaster Ave, Villanova, PA 19085 USA.
EM andrej.prsa@villanova.edu
RI Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Conroy, Kyle/0000-0002-5442-8550
FU NASA/Caltech [2-1085696]; NSF RUI [AST-05-07542]; NASA [NNX08AR15G,
NNX08AR14G]
FX This work is funded in part by the NASA/Caltech subcontract 2-1085696
(PI:Prsa) and NSF RUI AST-05-07542. L.R.D. and R.W.S. are supported by
the Kepler Mission Participating Scientist Program, NASA grant
NNX08AR15G awarded to L.R.D. W.F.W. acknowledges support from the Kepler
Participating Scientists Program via NASA grant NNX08AR14G.
NR 62
TC 185
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U1 1
U2 11
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 MAR
PY 2011
VL 141
IS 3
AR 83
DI 10.1088/0004-6256/141/3/83
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 719TC
UT WOS:000287231000014
ER
PT J
AU Southworth, J
Dominik, M
Jorgensen, UG
Rahvar, S
Snodgrass, C
Alsubai, K
Bozza, V
Browne, P
Burgdorf, M
Novati, SC
Dodds, P
Dreizler, S
Finet, F
Gerner, T
Hardis, S
Harpsoe, K
Hellier, C
Hinse, TC
Hundertmark, M
Kains, N
Kerins, E
Liebig, C
Mancini, L
Mathiasen, M
Penny, MT
Proft, S
Ricci, D
Sahu, K
Scarpetta, G
Schafer, S
Schonebeck, F
Surdej, J
AF Southworth, J.
Dominik, M.
Jorgensen, U. G.
Rahvar, S.
Snodgrass, C.
Alsubai, K.
Bozza, V.
Browne, P.
Burgdorf, M.
Novati, S. Calchi
Dodds, P.
Dreizler, S.
Finet, F.
Gerner, T.
Hardis, S.
Harpsoe, K.
Hellier, C.
Hinse, T. C.
Hundertmark, M.
Kains, N.
Kerins, E.
Liebig, C.
Mancini, L.
Mathiasen, M.
Penny, M. T.
Proft, S.
Ricci, D.
Sahu, K.
Scarpetta, G.
Schaefer, S.
Schoenebeck, F.
Surdej, J.
TI A much lower density for the transiting extrasolar planet WASP-7
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: fundamental parameters; planetary systems;
stars: individual: WASP-7
ID STELLAR EVOLUTION DATABASE; HIGH-PRECISION PHOTOMETRY; ECLIPSING
BINARIES; SURFACE GRAVITIES; LIGHT CURVES; MODELS; ISOCHRONES; STAR;
METALLICITY; EXOPLANETS
AB We present the first high-precision photometry of the transiting extrasolar planetary system WASP-7, obtained using telescope defocussing techniques and reaching a scatter of 0.68 mmag per point. We find that the transit depth is greater and that the host star is more evolved than previously thought. The planet has a significantly larger radius (1.330 +/- 0.093 R(Jup) versus 0.915(-0.040)(+0.046) R(Jup)) and much lower density (0.41 +/- 0.10 rho(Jup) versus 1.26(-0.21)(+0.25) rho(Jup)) and surface gravity (13.4 +/- 2.6 ms(-2) versus 26.4(-4.0)(+4.4) ms(-2)) than previous measurements showed. Based on the revised properties it is no longer an outlier in planetary mass-radius and period-gravity diagrams. We also obtain a more precise transit ephemeris for the WASP-7 system.
C1 [Southworth, J.; Hellier, C.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Dominik, M.; Browne, P.; Dodds, P.; Kains, N.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Jorgensen, U. G.; Hardis, S.; Harpsoe, K.; Hinse, T. C.; Mathiasen, M.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Jorgensen, U. G.; Hardis, S.; Harpsoe, K.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Snodgrass, C.] European So Observ, Santiago 19, Chile.
[Alsubai, K.] Qatar Fdn, Doha, Qatar.
[Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
[Burgdorf, M.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Burgdorf, M.] NASA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, I-80125 Naples, Italy.
[Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] IIASS, I-84019 Vietri Sur Mare, SA, Italy.
[Dreizler, S.; Hundertmark, M.; Schaefer, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Kains, N.] European So Observ, D-85748 Garching, Germany.
[Finet, F.; Ricci, D.; Surdej, J.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Gerner, T.; Proft, S.; Schoenebeck, F.] Univ Heidelberg, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Kerins, E.; Penny, M. T.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Mancini, L.] Univ Sannio, Dipartimento Ingn, I-82100 Benevento, Italy.
[Sahu, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Southworth, J (reprint author), Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
EM jkt@astro.keele.ac.uk
RI Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008;
OI Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Penny,
Matthew/0000-0001-7506-5640; Snodgrass, Colin/0000-0001-9328-2905
FU STFC; Department of Culture, Arts & Leisure (DCAL).; Communaute
francaise de Belgique - Actions de recherche concertees - Academie
Wallonie-Europe
FX J.S. acknowledges funding from STFC in the form of an Advanced
Fellowship. We thank the referee for comments which helped to improve
the paper. Astronomical research at Armagh Observatory is funded by the
Department of Culture, Arts & Leisure (DCAL). J. Surdej, D. R. (boursier
FRIA) and F. F. acknowledge support from the Communaute francaise de
Belgique - Actions de recherche concertees - Academie Wallonie-Europe.
NR 29
TC 11
Z9 11
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2011
VL 527
AR A8
DI 10.1051/0004-6361/201016183
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 723CP
UT WOS:000287484100023
ER
PT J
AU Batalha, NM
Borucki, WJ
Bryson, ST
Buchhave, LA
Caldwell, DA
Christensen-Dalsgaard, J
Ciardi, D
Dunham, EW
Fressin, F
Gautier, TN
Gilliland, RL
Haas, MR
Howell, SB
Jenkins, JM
Kjeldsen, H
Koch, DG
Latham, DW
Lissauer, JJ
Marcy, GW
Rowe, JF
Sasselov, DD
Seager, S
Steffen, JH
Torres, G
Basri, GS
Brown, TM
Charbonneau, D
Christiansen, J
Clarke, B
Cochran, WD
Dupree, A
Fabrycky, DC
Fischer, D
Ford, EB
Fortney, J
Girouard, FR
Holman, MJ
Johnson, J
Isaacson, H
Klaus, TC
Machalek, P
Moorehead, AV
Morehead, RC
Ragozzine, D
Tenenbaum, P
Twicken, J
Quinn, S
VanCleve, J
Walkowicz, LM
Welsh, WF
Devore, E
Gould, A
AF Batalha, Natalie M.
Borucki, William J.
Bryson, Stephen T.
Buchhave, Lars A.
Caldwell, Douglas A.
Christensen-Dalsgaard, Jorgen
Ciardi, David
Dunham, Edward W.
Fressin, Francois
Gautier, Thomas N., III
Gilliland, Ronald L.
Haas, Michael R.
Howell, Steve B.
Jenkins, Jon M.
Kjeldsen, Hans
Koch, David G.
Latham, David W.
Lissauer, Jack J.
Marcy, Geoffrey W.
Rowe, Jason F.
Sasselov, Dimitar D.
Seager, Sara
Steffen, Jason H.
Torres, Guillermo
Basri, Gibor S.
Brown, Timothy M.
Charbonneau, David
Christiansen, Jessie
Clarke, Bruce
Cochran, William D.
Dupree, Andrea
Fabrycky, Daniel C.
Fischer, Debra
Ford, Eric B.
Fortney, Jonathan
Girouard, Forrest R.
Holman, Matthew J.
Johnson, John
Isaacson, Howard
Klaus, Todd C.
Machalek, Pavel
Moorehead, Althea V.
Morehead, Robert C.
Ragozzine, Darin
Tenenbaum, Peter
Twicken, Joseph
Quinn, Samuel
VanCleve, Jeffrey
Walkowicz, Lucianne M.
Welsh, William F.
Devore, Edna
Gould, Alan
TI KEPLER'S FIRST ROCKY PLANET: KEPLER-10b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (Kepler-10 KIC 11904151, 2MASS
19024305+5014286); techniques: photometric; techniques: spectroscopic
ID MASS-RADIUS RELATIONSHIPS; TESTING BLEND SCENARIOS; LIGHT CURVES;
INITIAL CHARACTERISTICS; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS;
SUPER-EARTHS; CADENCE DATA; EXOPLANET; STARS
AB NASA's Kepler Mission uses transit photometry to determine the frequency of Earth-size planets in or near the habitable zone of Sun-like stars. The mission reached a milestone toward meeting that goal: the discovery of its first rocky planet, Kepler-10b. Two distinct sets of transit events were detected: (1) a 152 +/- 4 ppm dimming lasting 1.811 +/- 0.024 hr with ephemeris T [BJD] = 2454964.57375(-0.00082)(+0.00060) + N * 0.837495(-0.000005)(+0.000004) days and (2) a 376 +/- 9 ppm dimming lasting 6.86 +/- 0.07 hr with ephemeris T [BJD] = 2454971.6761(-0.0023)(+0.0020) + N * 45.29485(-0.00076)(+0.00065) days. Statistical tests on the photometric and pixel flux time series established the viability of the planet candidates triggering ground-based follow-up observations. Forty precision Doppler measurements were used to confirm that the short-period transit event is due to a planetary companion. The parent star is bright enough for asteroseismic analysis. Photometry was collected at 1 minute cadence for > 4 months from which we detected 19 distinct pulsation frequencies. Modeling the frequencies resulted in precise knowledge of the fundamental stellar properties. Kepler-10 is a relatively old (11.9 +/- 4.5 Gyr) but otherwise Sun-like main-sequence star with T-eff = 5627 +/- 44 K, M-star = 0.895 +/- 0.060M(circle dot), and R-star = 1.056 +/- 0.021R(circle dot). Physical models simultaneously fit to the transit light curves and the precision Doppler measurements yielded tight constraints on the properties of Kepler-10b that speak to its rocky composition: M-P = 4.56(-1.29)(+1.17) M-circle plus, R-P = 1.416(-0.036)(+0.033) R-circle plus, and rho P = 8.8(-2.9)(+2.1) g cm(-3). Kepler-10b is the smallest transiting exoplanet discovered to date.
C1 [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Caldwell, Douglas A.; Jenkins, Jon M.; Clarke, Bruce; Machalek, Pavel; Tenenbaum, Peter; Twicken, Joseph; VanCleve, Jeffrey; Devore, Edna] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Buchhave, Lars A.; Fressin, Francois; Latham, David W.; Sasselov, Dimitar D.; Torres, Guillermo; Charbonneau, David; Dupree, Andrea; Fabrycky, Daniel C.; Holman, Matthew J.; Ragozzine, Darin; Quinn, Samuel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[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.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Marcy, Geoffrey W.; Basri, Gibor S.; Isaacson, Howard; Walkowicz, Lucianne M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Seager, Sara] MIT, Cambridge, MA 02139 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06510 USA.
[Ford, Eric B.; Moorehead, Althea V.; Morehead, Robert C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Girouard, Forrest R.; Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA.
RP Batalha, NM (reprint author), San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
EM Natalie.Batalha@sjsu.edu
RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; 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 National Science Foundation; NASA's Science Mission Directorate
FX The authors thank Carly Chubak for computing the barycentric radial
velocity of Kepler-10. J.C.D. acknowledges support from The National
Center for Atmospheric Research which is sponsored by the National
Science Foundation. Funding for this Discovery mission is provided by
NASA's Science Mission Directorate.
NR 81
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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 MAR 1
PY 2011
VL 729
IS 1
AR 27
DI 10.1088/0004-637X/729/1/27
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300027
ER
PT J
AU Bhat, NDR
Andersson, BG
AF Bhat, N. D. R.
Andersson, B-G
TI ON THE MAGNETIC FIELD THROUGH THE UPPER CENTAURUS-LUPUS SUPER BUBBLE IN
THE VICINITY OF THE SOUTHERN COALSACK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (Southern Coalsack); ISM: magnetic fields;
pulsars: general; pulsars: individual (PSR J1047-6709, PSR J1210-6550,
PSR J1435-5954)
ID PULSAR ROTATION MEASURES; SCORPIO-CENTAURUS; GALACTIC PLANE; DUSTY RING;
2.4 GHZ; X-RAY; CLOUDS; SUPERBUBBLES; SIMULATIONS; DISCOVERY
AB The Southern Coalsack is located in the interior of the Upper Centaurus-Lupus (UCL) super bubble and shows many traits that point to a much more energetic environment than might be expected from a dark, starless molecular cloud. A hot, X-ray emitting envelope surrounds the cloud, it has a very strong internal magnetic field, and its darkest core seems to be on astronomical timescales "just about" to start forming stars. In order to probe the magnetic environment of the cloud and to compare with the optical/near-infrared polarimetry-based field estimates for the cloud, we have acquired Faraday rotation measurements toward the pulsar PSR J1210-6550, probing the magnetic field in the vicinity of the cloud, and a comparison target, PSR J1435-5954, at a similar line-of-sight distance but several degrees from the cloud. Both lines of sight hence primarily probe the UCL super bubble. The earlier estimates of the magnetic field inside the Coalsack, using the Chandrasekhar-Fermi method on optical and near-infrared polarimetry, yield B-perpendicular to = 64-93 mu G. However, even though PSR J1210-6550 is located only similar to 30 arcmin from the (CO) edge of the cloud, the measured field strength is only B-parallel to = -1.1 +/- 0.2 mu G. While thus yielding a very high field contrast to the cloud we argue that this might be understood as due to the effects on the cloud by the super bubble.
C1 [Bhat, N. D. R.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Andersson, B-G] NASA, Ames Res Ctr, SOFIA Sci Ctr USRA, Moffett Field, CA 94035 USA.
RP Bhat, NDR (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
RI Bhat, Ramesh/B-7396-2013;
OI Andersson, B-G/0000-0001-6717-0686
FU Commonwealth of Australia
FX We are grateful to Willem van Straten and Aristeidis Noutsos for
discussions on the polarimetric analysis, Ravi Sankrit and Tim Robishaw
for discussions on the super bubble models and interstellar magnetic
fields, and Matthew Bailes for his encouragement and support to this
project. We thank an anonymous referee who provided useful comments that
helped to improve the paper. The Parkes radio telescope is part of the
Australia Telescope, which is funded by the Commonwealth of Australia
for operation as a National Facility managed by the Commonwealth
Scientific and Industrial Research Organization.
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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 MAR 1
PY 2011
VL 729
IS 1
AR 38
DI 10.1088/0004-637X/729/1/38
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300038
ER
PT J
AU Debes, JH
Hoard, DW
Kilic, M
Wachter, S
Leisawitz, DT
Cohen, M
Kirkpatrick, JD
Griffith, RL
AF Debes, John H.
Hoard, D. W.
Kilic, Mukremin
Wachter, Stefanie
Leisawitz, David T.
Cohen, Martin
Kirkpatrick, J. Davy
Griffith, Roger L.
TI THE WIRED SURVEY. I. A BRIGHT IR EXCESS DUE TO DUST AROUND THE HEAVILY
POLLUTED WHITE DWARF GALEX J193156.8+011745
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; white dwarfs
ID ALL-SKY SURVEY; SPITZER-SPACE-TELESCOPE; GASEOUS DEBRIS DISC; SOURCE
INFRARED SKY; PLANETARY SYSTEMS; STELLAR EVOLUTION; MU-M; G29-38;
ACCRETION; CATALOG
AB With the launch of the Wide-Field Infrared Survey Explorer (WISE), a new era of detecting planetary debris around white dwarfs (WDs) has begun with the WISE InfraRed Excesses around Degenerates (WIRED) Survey. The WIRED survey will be sensitive to substellar objects and dusty debris around WDs out to distances exceeding 100 pc, well beyond the completeness level of local WDs and covering a large fraction of known WDs detected with the SDSS DR4 WD catalog. In this paper, we report an initial result of the WIRED survey, the detection of the heavily polluted hydrogen WD (spectral type DAZ) GALEX J193156.8+011745 at 3.35 and 4.6 mu m. We find that the excess is consistent with either a narrow dusty ring with an inner radius of 29 R-WD, outer radius of 40 R-WD, and a face-on inclination, or a disk with an inclination of 70 degrees, an inner radius of 23 R-WD, and an outer radius of 80 R-WD. We also report initial optical spectroscopic monitoring of several metal lines present in the photosphere and find no variability in the line strengths or radial velocities of the lines. We rule out all but planetary mass companions to GALEX1931 out to 0.5 AU.
C1 [Debes, John H.; Leisawitz, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Kilic, Mukremin] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Wachter, Stefanie; Kirkpatrick, J. Davy; Griffith, Roger L.] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Cohen, Martin] Monterey Inst Res Astron, Marina, CA 93933 USA.
RP Debes, JH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
OI Hoard, Donald W./0000-0002-6800-6519
FU NASA; National Science Foundation; NASA through UCLA [1000-S-MA756];
UCLA [FAU 26311]
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. This work is based
on data obtained from (1) the Wide-Field Infrared Survey Explorer, which
is a joint project of the University of California, Los Angeles, and the
Jet Propulsion Laboratory (JPL), California Institute of Technology
(Caltech), funded by the National Aeronautics and Space Administration
(NASA); (2) the Two Micron All Sky Survey, a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center (IPAC)/Caltech, funded by NASA and the National Science
Foundation; (3) the Hale Telescope, Palomar Observatory, as part of a
continuing collaboration between Caltech, NASA/JPL, and Cornell
University; (4) the 6.5 m Magellan Telescopes located at Las Campanas
Observatory, Chile; (5) the ESO Telescopes at the La Silla or Paranal
Observatories; (6) the SIMBAD database, operated at CDS, Strasbourg,
France; and (7) the NASA/IPAC Infrared Science Archive, which is
operated by JPL, Caltech, under a contract with NASA. We thank D.
Steeghs for obtaining spectra of GALEX1931 on July 7-8 and N. Morrell
for obtaining spectra of GALEX1931 on August 2-3. M. C. thanks NASA for
supporting his participation in this work through UCLA Sub-Award
1000-S-MA756 with a UCLA FAU 26311 to MIRA.
NR 50
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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 MAR 1
PY 2011
VL 729
IS 1
AR 4
DI 10.1088/0004-637X/729/1/4
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300004
ER
PT J
AU Kim, YS
Kaiser, RI
AF Kim, Y. S.
Kaiser, R. I.
TI ON THE FORMATION OF AMINES (RNH2) AND THE CYANIDE ANION (CN-) IN
ELECTRON-IRRADIATED AMMONIA-HYDROCARBON INTERSTELLAR MODEL ICES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; astrochemistry; cosmic rays; ISM: individual objects
(Sagittarius B2); ISM: molecules; methods: laboratory
ID SOLAR-SYSTEM; LOW-TEMPERATURE; ANALOG ICES; LINE SURVEY; COMETARY;
METHYLAMINE; MOLECULES; CHEMISTRY; GLYCINE; METHANE
AB The present laboratory study simulated cosmic-ray-induced grain chemistry of nitrogen-bearing organic molecules in interstellar and cometary ices. Model ices of ammonia (NH3)-methane (CH4) were prepared and irradiated at 10 K under contamination-free, ultrahigh vacuum conditions with energetic electrons generated in the track of galactic cosmic-ray particles. The radiolysis-induced processing of nitrogen-bearing molecules was then monitored on line and in situ by a Fourier transform infrared spectrometer and a quadrupole mass spectrometer during the irradiation phase and subsequent warm-up phases. The analogous processing was also achieved in ammonia (NH3) and six hydrocarbon (CnH2n+2; n = 1-6) ices. The formation of cyanide anion (CN-) was commonly observed in both ices at 10 K, the temporal column density fit of which traced back the involvement of methylamine (CH3NH2)-based intermediates. Traces of CH3NH2 were evident at about 110 K through thin ammonia matrices in sublimation. From the point of radiative transfer, we further constrain the formationmechanism of aminoacetonitrile (NH2CH2CN) on icy grains of Sgr B-2(N) under a cosmic-ray-induced photon field.
C1 [Kim, Y. S.; Kaiser, R. I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Kaiser, R. I.] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
RP Kim, YS (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
EM ralfk@hawaii.edu
FU National Aeronautics Space Administration (NASA) Astrobiology Institute
through the Office of Space Science [NNA09DA77A]
FX This work was supported by the National Aeronautics Space Administration
(NASA) Astrobiology Institute under Cooperative Agreement no. NNA09DA77A
issued through the Office of Space Science. Special thanks to C. S.
Jamieson (University of Hawaii) and P. D. Holtom (The Open University)
for preparing the methane-ammonia and methylamine ices, respectively. We
also acknowledge Dr. C. Ennis (University of Hawaii) for proofreading
this manuscript.
NR 48
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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 MAR 1
PY 2011
VL 729
IS 1
AR 68
DI 10.1088/0004-637X/729/1/68
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 720BN
UT WOS:000287255300068
ER
PT J
AU Marshall, HL
Gelbord, JM
Schwartz, DA
Murphy, DW
Lovell, JEJ
Worrall, DM
Birkinshaw, M
Perlman, ES
Godfrey, L
Jauncey, DL
AF Marshall, H. L.
Gelbord, J. M.
Schwartz, D. A.
Murphy, D. W.
Lovell, J. E. J.
Worrall, D. M.
Birkinshaw, M.
Perlman, E. S.
Godfrey, L.
Jauncey, D. L.
TI AN X-RAY IMAGING SURVEY OF QUASAR JETS: TESTING THE INVERSE COMPTON
MODEL
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: active; galaxies: jets; surveys
ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; HEMISPHERE ICRF SOURCES;
DOMINATED RADIO-SOURCES; LARGE-SCALE JETS; VLBI OBSERVATIONS; COMPLETE
SAMPLE; CHANDRA OBSERVATIONS; RELATIVISTIC JETS; VLA OBSERVATIONS
AB We present results from continued Chandra X-ray imaging and spectroscopy of a flux-limited sample of flat spectrum radio-emitting quasars with jet-like extended structure. X-rays are detected from 24 of the 39 jets observed so far. We compute the distribution of alpha(rx), the spectral index between the X-ray and radio bands, showing that it is broad, extending at least from 0.8 to 1.2. While there is a general trend that the radio brightest jets are detected most often, it is clear that predicting the X-ray flux from the radio knot flux densities is risky, so a shallow X-ray survey is the most effective means for finding jets that are X-ray bright. We test the model in which the X-rays result from inverse Compton (IC) scattering of cosmic microwave background (CMB) photons by relativistic electrons in the jet moving with a high bulk Lorentz factor nearly along the line of sight. Depending on how the jet magnetic fields vary with z, the observed X-ray to radio flux ratios do not follow the redshift dependence expected from the IC-CMB model. For a subset of our sample with known superluminal motion based on VLBI observations, we estimate the angle of the kiloparsec-scale jet to the line of sight by considering the additional information in the bends observed between parsec-and kiloparsec-scale jets. These angles are sometimes much smaller than estimates based on the IC-CMB model with a Lorentz factor of 15, indicating that these jets may decelerate significantly from parsec scales to kiloparsec scales.
C1 [Marshall, H. L.; Gelbord, J. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Gelbord, J. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Gelbord, J. M.] Penn State Univ, Dept Astron & Astrophys, State Coll, PA 16801 USA.
[Schwartz, D. A.; Worrall, D. M.; Birkinshaw, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Murphy, D. W.; Godfrey, L.; Jauncey, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lovell, J. E. J.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Worrall, D. M.; Birkinshaw, M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England.
[Perlman, E. S.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Perlman, E. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Godfrey, L.] Curtin Univ Technol, Curtin Inst Radio Astron, Bentley, WA 6845, Australia.
RP Marshall, HL (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM hermanm@space.mit.edu; jgelbord@astro.psu.edu; das@head-cfa.harvard.edu;
david.murphy@jpl.nasa.gov; jim.lovell@utas.edu.au;
D.Worrall@bristol.ac.uk; Mark.Birkinshaw@bristol.ac.uk;
eperlman@fit.edu; L.Godfrey@curtin.edu.au; David.Jauncey@csiro.au
RI Godfrey, Leith/B-5283-2013
FU National Aeronautics and Space Administration (NASA) through the
Smithsonian Astrophysical Observatory (SAO) [SV3-73016]; NASA
[NAS8-03060, NAS 8-39073]; CXC [GO4-5124X]; Commonwealth of Australia
for operation as a National Facility
FX We thank Marshall Cohen for communicating results in advance of
publication. Support for this work was provided in part by the National
Aeronautics and Space Administration (NASA) through the Smithsonian
Astrophysical Observatory (SAO) contract SV3-73016 to MIT for support of
the Chandra X-Ray Center (CXC), which is operated by SAO for and on
behalf of NASA under contract NAS8-03060. Support was also provided by
NASA under contract NAS 8-39073 to SAO. J.M.G. was partially supported
under Chandra grant GO4-5124X to MIT from the CXC. This research has
made use of data from the MOJAVE database that is maintained by the
MOJAVE team (Lister et al. 2009a). This research has made use of the
United States Naval Observatory (USNO) Radio Reference Frame Image
Database (RRFID). 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. This research has
made use of the NASA/IPAC Extragalactic Database (NED) which is operated
by the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
NR 50
TC 17
Z9 18
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2011
VL 193
IS 1
DI 10.1088/0067-0049/193/1/15
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 743ZF
UT WOS:000289059000015
ER
PT J
AU Csepp, DJ
Vollenweider, JJ
Sigler, MF
AF Csepp, David J.
Vollenweider, Johanna J.
Sigler, Michael F.
TI Seasonal abundance and distribution of pelagic and demersal fishes in
southeastern Alaska
SO FISHERIES RESEARCH
LA English
DT Article
DE Echo integration-trawl survey; Acoustics; Long line survey; Pelagic;
Demersal; Walleye pollock; Theragra chalcogramma; Pacific hake;
Merluccius productus; Pacific herring; Clupea pallasii
ID STELLER SEA LIONS; POLLOCK THERAGRA-CHALCOGRAMMA; EULACHON
THALEICHTHYS-PACIFICUS; SABLEFISH ANOPLOPOMA-FIMBRIA; TARGET-STRENGTH
MEASUREMENTS; DIEL VERTICAL MIGRATION; WALLEYE POLLOCK;
EUMETOPIAS-JUBATUS; BERING-SEA; MERLUCCIUS-PRODUCTUS
AB We quantified seasonal and interannual variability of pelagic and demersal fishes available to marine predators in southeastern Alaska focusing on prey of the Steller sea lion (Eumetopias jubatus). Estimates of abundance were determined from echo integration mid-water trawl and demersal longline surveys. The dominant species were walleye pollock (Theragra chalcogramma) (average biomass 9057 t). Pacific hake (Merluccius productus) (1715 t), Pacific herring (Clupea pallasii) (1176 t), Pacific halibut (Hippoglossus srenolepis) (average catch rate 524 kg per 1000 hooks), Pacific cod (Gadus macrocephalus) (177 kg per 1000 hooks), sablefish (Anoplopoma fimbria) (120 kg per 1000 hooks), and sandpaper skate (Bathyraja interrupta) (26 kg per 1000 hooks). Of these species, seasonal differences in species abundance were detected for walleye pollock (p = 0.03), Pacific cod (p = 0.001) and sablefish (p < 0.001) with walleye pollock the most abundant and widespread species year-round. Herring, hake, and juvenile (120-350 mm) and adult (>350 mm) pollock are pelagic species. Adult and juvenile pollock and hake were found in open water, while herring, young-of-the-year (<120 mm) and the smallest juvenile pollock were found in bays. H erring of all ages concentrate in dense schools. Pollock and hake form scattered layers throughout open water with juvenile pollock shallower than adult pollock and adult pollock shallower than hake. Halibut, sablefish, skates, Pacific cod and arrowtooth flounder are demersal species; sablefish were deeper than the other demersal species. These seasonal and annual changes in prey availability affected prey selection of sea lions which shifted their diet in response. Published by Elsevier B.V.
C1 [Csepp, David J.; Vollenweider, Johanna J.; Sigler, Michael F.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Ted Stevens Marine Res Inst, Juneau, AK 99801 USA.
RP Csepp, DJ (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Ted Stevens Marine Res Inst, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA.
EM Dave.Csepp@noaa.gov
RI Bizzarro, Joseph/A-2988-2012
NR 63
TC 5
Z9 5
U1 3
U2 30
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-7836
J9 FISH RES
JI Fish Res.
PD MAR
PY 2011
VL 108
IS 2-3
BP 307
EP 320
DI 10.1016/j.fishres.2011.01.003
PG 14
WC Fisheries
SC Fisheries
GA 738LF
UT WOS:000288640600010
ER
EF