FN Thomson Reuters Web of Science™
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PT J
AU Aghanim, N
Arnaud, M
Ashdown, M
Aumont, J
Baccigalupi, C
Balbi, A
Banday, AJ
Barreiro, RB
Bartelmann, M
Bartlett, JG
Battaner, E
Benabed, K
Benoit, A
Bernard, JP
Bersanelli, M
Bhatia, R
Bock, JJ
Bonaldi, A
Bond, JR
Borrill, J
Bouchet, FR
Brown, ML
Bucher, M
Burigana, C
Cabella, P
Cardoso, JF
Catalano, A
Cayon, L
Challinor, A
Chamballu, A
Chiang, LY
Chiang, C
Chon, G
Christensen, PR
Churazov, E
Clements, DL
Colafrancesco, S
Colombi, S
Couchot, F
Coulais, A
Crill, BP
Cuttaia, F
Da Silva, A
Dahle, H
Danese, L
Davis, RJ
de Bernardis, P
de Gasperis, G
de Rosa, A
de Zotti, G
Delabrouille, J
Delouis, JM
Desert, FX
Diego, JM
Dolag, K
Donzelli, S
Dore, O
Dorl, U
Douspis, M
Dupac, X
Efstathiou, G
Ensslin, TA
Finelli, F
Flores-Cacho, I
Forni, O
Frailis, M
Franceschi, E
Fromenteau, S
Galeotta, S
Ganga, K
Genova-Santos, RT
Giard, M
Giardino, G
Giraud-Heraud, Y
Gonzalez-Nuevo, J
Gorski, KM
Gratton, S
Gregorio, A
Gruppuso, A
Harrison, D
Henrot-Versille, S
Hernandez-Monteagudo, C
Herranz, D
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hovest, W
Hoyland, RJ
Huffenberger, KM
Jaffe, AH
Jones, WC
Juvela, M
Keihanen, E
Keskitalo, R
Kisner, TS
Kneissl, R
Knox, L
Kurki-Suonio, H
Lagache, G
Lamarre, JM
Lasenby, A
Laureijs, RJ
Lawrence, CR
Leach, S
Leonardi, R
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Macias-Perez, JF
MacTavish, CJ
Maffei, B
Maino, D
Mandolesi, N
Mann, R
Maris, M
Marleau, F
Martinez-Gonzalez, E
Masi, S
Matarrese, S
Matthai, F
Mazzotta, P
Mei, S
Melchiorri, A
Melin, JB
Mendes, L
Mennella, A
Mitra, S
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, A
Naselsky, P
Natoli, P
Netterfield, CB
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
O'Dwyer, IJ
Osborne, S
Pajot, F
Pasian, F
Patanchon, G
Perdereau, O
Perotto, L
Perrotta, F
Piacentini, F
Piat, M
Pierpaoli, E
Piffaretti, R
Plaszczynski, S
Pointecouteau, E
Polenta, G
Ponthieu, N
Poutanen, T
Pratt, GW
Prezeau, G
Prunet, S
Puget, JL
Rebolo, R
Reinecke, M
Renault, C
Ricciardi, S
Riller, T
Ristorcelli, I
Rocha, G
Rosset, C
Rubino-Martin, JA
Rusholme, B
Sandri, M
Savini, G
Schaefer, BM
Scott, D
Seiffert, MD
Shellard, P
Smoot, GF
Starck, JL
Stivoli, F
Stolyarov, V
Sudiwala, R
Sunyaev, R
Sygnet, JF
Tauber, JA
Terenzi, L
Toffolatti, L
Tomasi, M
Torre, JP
Tristram, M
Tuovinen, J
Valenziano, L
Vibert, L
Vielva, P
Villa, F
Vittorio, N
Wandelt, BD
White, SDM
White, M
Yvon, D
Zacchei, A
Zonca, A
AF Aghanim, N.
Arnaud, M.
Ashdown, M.
Aumont, J.
Baccigalupi, C.
Balbi, A.
Banday, A. J.
Barreiro, R. B.
Bartelmann, M.
Bartlett, J. G.
Battaner, E.
Benabed, K.
Benoit, A.
Bernard, J-P.
Bersanelli, M.
Bhatia, R.
Bock, J. J.
Bonaldi, A.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Brown, M. L.
Bucher, M.
Burigana, C.
Cabella, P.
Cardoso, J-F.
Catalano, A.
Cayon, L.
Challinor, A.
Chamballu, A.
Chiang, L-Y
Chiang, C.
Chon, G.
Christensen, P. R.
Churazov, E.
Clements, D. L.
Colafrancesco, S.
Colombi, S.
Couchot, F.
Coulais, A.
Crill, B. P.
Cuttaia, F.
Da Silva, A.
Dahle, H.
Danese, L.
Davis, R. J.
de Bernardis, P.
de Gasperis, G.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Delouis, J-M.
Desert, F-X.
Diego, J. M.
Dolag, K.
Donzelli, S.
Dore, O.
Doerl, U.
Douspis, M.
Dupac, X.
Efstathiou, G.
Ensslin, T. A.
Finelli, F.
Flores-Cacho, I.
Forni, O.
Frailis, M.
Franceschi, E.
Fromenteau, S.
Galeotta, S.
Ganga, K.
Genova-Santos, R. T.
Giard, M.
Giardino, G.
Giraud-Heraud, Y.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gratton, S.
Gregorio, A.
Gruppuso, A.
Harrison, D.
Henrot-Versille, S.
Hernandez-Monteagudo, C.
Herranz, D.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Holmes, W. A.
Hovest, W.
Hoyland, R. J.
Huffenberger, K. M.
Jaffe, A. H.
Jones, W. C.
Juvela, M.
Keihanen, E.
Keskitalo, R.
Kisner, T. S.
Kneissl, R.
Knox, L.
Kurki-Suonio, H.
Lagache, G.
Lamarre, J-M.
Lasenby, A.
Laureijs, R. J.
Lawrence, C. R.
Leach, S.
Leonardi, R.
Linden-Vornle, M.
Lopez-Caniego, M.
Lubin, P. M.
Macias-Perez, J. F.
MacTavish, C. J.
Maffei, B.
Maino, D.
Mandolesi, N.
Mann, R.
Maris, M.
Marleau, F.
Martinez-Gonzalez, E.
Masi, S.
Matarrese, S.
Matthai, F.
Mazzotta, P.
Mei, S.
Melchiorri, A.
Melin, J-B.
Mendes, L.
Mennella, A.
Mitra, S.
Miville-Deschenes, M-A.
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Murphy, A.
Naselsky, P.
Natoli, P.
Netterfield, C. B.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
O'Dwyer, I. J.
Osborne, S.
Pajot, F.
Pasian, F.
Patanchon, G.
Perdereau, O.
Perotto, L.
Perrotta, F.
Piacentini, F.
Piat, M.
Pierpaoli, E.
Piffaretti, R.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Ponthieu, N.
Poutanen, T.
Pratt, G. W.
Prezeau, G.
Prunet, S.
Puget, J-L.
Rebolo, R.
Reinecke, M.
Renault, C.
Ricciardi, S.
Riller, T.
Ristorcelli, I.
Rocha, G.
Rosset, C.
Rubino-Martin, J. A.
Rusholme, B.
Sandri, M.
Savini, G.
Schaefer, B. M.
Scott, D.
Seiffert, M. D.
Shellard, P.
Smoot, G. F.
Starck, J-L.
Stivoli, F.
Stolyarov, V.
Sudiwala, R.
Sunyaev, R.
Sygnet, J-F.
Tauber, J. A.
Terenzi, L.
Toffolatti, L.
Tomasi, M.
Torre, J-P.
Tristram, M.
Tuovinen, J.
Valenziano, L.
Vibert, L.
Vielva, P.
Villa, F.
Vittorio, N.
Wandelt, B. D.
White, S. D. M.
White, M.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck early results. XII. Cluster Sunyaev-Zeldovich optical scaling
relations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: clusters: intracluster medium; cosmic background radiation;
large-scale structure of Universe; cosmology: observations; galaxies:
clusters: general
ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; PRE-LAUNCH STATUS; GALAXY
CLUSTERS; RICHNESS RELATION; L-X; CATALOG; COSMOLOGY; MAXBCG; SAMPLE
AB We present the Sunyaev-Zeldovich (SZ) signal-to-richness scaling relation (Y-500 - N-200) for the MaxBCG cluster catalogue. Employing a multi-frequency matched filter on the Planck sky maps, we measure the SZ signal for each cluster by adapting the filter according to weak-lensing calibrated mass-richness relations (N-200 - M-500). We bin our individual measurements and detect the SZ signal down to the lowest richness systems (N-200 = 10) with high significance, achieving a detection of the SZ signal in systems with mass as low as M-500 approximate to 5 x 10(13) M-circle dot. The observed Y-500 - N-200 relation is well modeled by a power law over the full richness range. It has a lower normalisation at given N-200 than predicted based on X-ray models and published mass-richness relations. An X-ray subsample, however, does conform to the predicted scaling, and model predictions do reproduce the relation between our measured bin-average SZ signal and measured bin-average X-ray luminosities. At fixed richness, we find an intrinsic dispersion in the Y-500 - N-200 relation of 60% rising to of order 100% at low richness. Thanks to its all-sky coverage, Planck provides observations for more than 13 000 MaxBCG clusters and an unprecedented SZ/optical data set, extending the list of known cluster scaling laws to include SZ-optical properties. The data set offers essential clues for models of galaxy formation. Moreover, the lower normalisation of the SZ-mass relation implied by the observed SZ-richness scaling has important consequences for cluster physics and cosmological studies with SZ clusters.
C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J-F.; Catalano, A.; Delabrouille, J.; Fromenteau, S.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR7164, F-75205 Paris 13, France.
[Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
[Ashdown, M.; Brown, M. L.; Chon, G.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile.
[Bond, J. R.; Miville-Deschenes, M-A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Banday, A. J.; Bernard, J-P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Dahle, H.] Univ Oslo, Ctr Math Applicat, Oslo, Norway.
[Da Silva, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Challinor, A.; Shellard, P.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England.
[Melin, J-B.; Piffaretti, R.; Starck, J-L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France.
[Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Marleau, F.; Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA.
[Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Smoot, G. F.; White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Leonardi, R.; Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
[Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
[Flores-Cacho, I.; Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain.
[Kneissl, R.] ESO Vitacura, European So Observ, Santiago, Chile.
[Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, Planck Sci Off, ESAC, Madrid, Spain.
[Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
[Mei, S.] Observ Paris, GEPI, Sect Meudon, F-92195 Meudon, France.
[Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland.
[Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy.
[Colafrancesco, S.; Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Maino, D.; Tomasi, M.] INAF IASF Milano, Milan, Italy.
[Stivoli, F.] Univ Paris 11, Lab Rech Informat, INRIA, F-91405 Orsay, France.
[Desert, F-X.] Univ Grenoble 1, IPAG, CNRS, INSU, F-38041 Grenoble, France.
[Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Ganga, K.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38041 Grenoble, France.
[Aghanim, N.; Aumont, J.; Douspis, M.; Fromenteau, S.; Lagache, G.; Miville-Deschenes, M-A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J-L.; Torre, J-P.; Vibert, L.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Benabed, K.; Bouchet, F. R.; Cardoso, J-F.; Colombi, S.; Delouis, J-M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J-F.; Wandelt, B. D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France.
[Chiang, L-Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Dahle, H.; Donzelli, S.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Flores-Cacho, I.; Genova-Santos, R. T.; Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Barreiro, R. B.; Diego, J. M.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; O'Dwyer, I. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Davis, R. J.; Maffei, B.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ashdown, M.; Brown, M. L.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Catalano, A.; Coulais, A.; Lamarre, J-M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
[Arnaud, M.; Piffaretti, R.; Pratt, G. W.; Starck, J-L.] Univ Paris Diderot, CNRS, CEA Saclay, Lab AIM,IRFU Serv Astrophys,CEA DSM, F-91191 Gif Sur Yvette, France.
[Cardoso, J-F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France.
[Cardoso, J-F.] Telecom ParisTech, F-75634 Paris 13, France.
[Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.] Univ Grenoble 1, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, CNRS,IN2P3, F-38026 Grenoble, France.
[Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, IN2P3, Lab Accelerateur Lineaire, F-91405 Orsay, France.
[Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Banday, A. J.; Bartelmann, M.; Churazov, E.; Dolag, K.; Doerl, U.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Chon, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland.
[Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland.
[Crill, B. P.] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA.
[Savini, G.] UCL, Opt Sci Lab, London, England.
[Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Mann, R.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Churazov, E.; Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Bartelmann, M.; Schaefer, B. M.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Banday, A. J.; Bernard, J-P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS, OMP, IRAP, F-31028 Toulouse 4, France.
[Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain.
[Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Bartlett, JG (reprint author), Univ Paris 07, CNRS, UMR7164, Batiment Condorcet,10 Rue A Domon & Leonie Duquet, F-75205 Paris 13, France.
EM bartlett@apc.univ-paris7.fr
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Eric/0000-0003-1880-2733; Savini, Giorgio/0000-0003-4449-9416;
Pierpaoli, Elena/0000-0002-7957-8993; Cuttaia,
Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099;
Burigana, Carlo/0000-0002-3005-5796; Bouchet,
Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X;
Galeotta, Samuele/0000-0002-3748-5115; TERENZI,
LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Pasian,
Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269;
Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840;
Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785;
Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375
FU CNES; CNRS; ASI; NASA; Danish Natural Research Council; CPAC at
Cambridge (UK); USPDC at IPAC (USA)
FX The authors from the consortia funded principally by CNES, CNRS, ASI,
NASA, and Danish Natural Research Council acknowledge the use of the
pipeline running infrastructures Magique3 at Institut d'Astrophysique de
Paris (France), CPAC at Cambridge (UK), and USPDC at IPAC (USA). We
acknowledge the use of the HEALPix package (Gorski et al. 2005). A
description of the Planck Collaboration and a list of its members,
indicating which technical or scientific activities they have been
involved in, can be found at http://www.rssd.esa.int/Planck.
NR 69
TC 86
Z9 86
U1 1
U2 7
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD DEC
PY 2011
VL 536
AR A12
DI 10.1051/0004-6361/201116489
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100013
ER
PT J
AU Aghanim, N
Arnaud, M
Ashdown, M
Aumont, J
Baccigalupi, C
Balbi, A
Banday, AJ
Barreiro, RB
Bartelmann, M
Bartlett, JG
Battaner, E
Benabed, K
Benoit, A
Bernard, JP
Bersanelli, M
Bhatia, R
Bock, JJ
Bonaldi, A
Bond, JR
Borrill, J
Bouchet, FR
Brown, ML
Bucher, M
Burigana, C
Cabella, P
Cardoso, JF
Catalano, A
Cayon, L
Challinor, A
Chamballu, A
Chary, RR
Chiang, LY
Chiang, C
Chon, G
Christensen, PR
Churazov, E
Clements, DL
Colafrancesco, S
Colombi, S
Couchot, F
Coulais, A
Crill, BP
Cuttaia, F
Da Silva, A
Dahle, H
Danese, L
de Bernardis, P
de Gasperis, G
de Rosa, A
de Zotti, G
Delabrouille, J
Delouis, JM
Desert, FX
Diego, JM
Dolag, K
Donzelli, S
Dore, O
Dorl, U
Douspis, M
Dupac, X
Efstathiou, G
Ensslin, TA
Finelli, F
Flores-Cacho, I
Forni, O
Frailis, M
Franceschi, E
Fromenteau, S
Galeotta, S
Ganga, K
Genova-Santos, RT
Giard, M
Giardino, G
Giraud-Heraud, Y
Gonzalez-Nuevo, J
Gorski, KM
Gratton, S
Gregorio, A
Gruppuso, A
Harrison, D
Henrot-Versille, S
Hernandez-Monteagudo, C
Herranz, D
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hovest, W
Hoyland, RJ
Huffenberger, KM
Jaffe, AH
Jones, WC
Juvela, M
Keihanen, E
Keskitalo, R
Kisner, TS
Kneissl, R
Knox, L
Kurki-Suonio, H
Lagache, G
Lamarre, JM
Lasenby, A
Laureijs, RJ
Lawrence, CR
Leach, S
Leonardi, R
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Macias-Perez, JF
MacTavish, CJ
Maffei, B
Maino, D
Mandolesi, N
Mann, R
Maris, M
Marleau, F
Martinez-Gonzalez, E
Masi, S
Matarrese, S
Matthai, F
Mazzotta, P
Melchiorri, A
Melin, JB
Mendes, L
Mennella, A
Mitra, S
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, A
Naselsky, P
Natoli, P
Netterfield, CB
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
Osborne, S
Pajot, F
Pasian, F
Patanchon, G
Perdereau, O
Perotto, L
Perrotta, F
Piacentini, F
Piat, M
Pierpaoli, E
Piffaretti, R
Plaszczynski, S
Pointecouteau, E
Polenta, G
Ponthieu, N
Poutanen, T
Pratt, GW
Prezeau, G
Prunet, S
Puget, JL
Rebolo, R
Reinecke, M
Renault, C
Ricciardi, S
Riller, T
Ristorcelli, I
Rocha, G
Rosset, C
Rubino-Martin, JA
Rusholme, B
Sandri, M
Santos, D
Schaefer, BM
Scott, D
Seiffert, MD
Smoot, GF
Starck, JL
Stivoli, F
Stolyarov, V
Sunyaev, R
Sygnet, JF
Tauber, JA
Terenzi, L
Toffolatti, L
Tomasi, M
Tristram, M
Tuovinen, J
Valenziano, L
Vibert, L
Vielva, P
Villa, F
Vittorio, N
Wandelt, BD
White, SDM
White, M
Yvon, D
Zacchei, A
Zonca, A
AF Aghanim, N.
Arnaud, M.
Ashdown, M.
Aumont, J.
Baccigalupi, C.
Balbi, A.
Banday, A. J.
Barreiro, R. B.
Bartelmann, M.
Bartlett, J. G.
Battaner, E.
Benabed, K.
Benoit, A.
Bernard, J. -P.
Bersanelli, M.
Bhatia, R.
Bock, J. J.
Bonaldi, A.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Brown, M. L.
Bucher, M.
Burigana, C.
Cabella, P.
Cardoso, J. -F.
Catalano, A.
Cayon, L.
Challinor, A.
Chamballu, A.
Chary, R. -R.
Chiang, L. -Y
Chiang, C.
Chon, G.
Christensen, P. R.
Churazov, E.
Clements, D. L.
Colafrancesco, S.
Colombi, S.
Couchot, F.
Coulais, A.
Crill, B. P.
Cuttaia, F.
Da Silva, A.
Dahle, H.
Danese, L.
de Bernardis, P.
de Gasperis, G.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Delouis, J. -M.
Desert, F. -X.
Diego, J. M.
Dolag, K.
Donzelli, S.
Dore, O.
Doerl, U.
Douspis, M.
Dupac, X.
Efstathiou, G.
Ensslin, T. A.
Finelli, F.
Flores-Cacho, I.
Forni, O.
Frailis, M.
Franceschi, E.
Fromenteau, S.
Galeotta, S.
Ganga, K.
Genova-Santos, R. T.
Giard, M.
Giardino, G.
Giraud-Heraud, Y.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gratton, S.
Gregorio, A.
Gruppuso, A.
Harrison, D.
Henrot-Versille, S.
Hernandez-Monteagudo, C.
Herranz, D.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Holmes, W. A.
Hovest, W.
Hoyland, R. J.
Huffenberger, K. M.
Jaffe, A. H.
Jones, W. C.
Juvela, M.
Keihanen, E.
Keskitalo, R.
Kisner, T. S.
Kneissl, R.
Knox, L.
Kurki-Suonio, H.
Lagache, G.
Lamarre, J. -M.
Lasenby, A.
Laureijs, R. J.
Lawrence, C. R.
Leach, S.
Leonardi, R.
Linden-Vornle, M.
Lopez-Caniego, M.
Lubin, P. M.
Macias-Perez, J. F.
MacTavish, C. J.
Maffei, B.
Maino, D.
Mandolesi, N.
Mann, R.
Maris, M.
Marleau, F.
Martinez-Gonzalez, E.
Masi, S.
Matarrese, S.
Matthai, F.
Mazzotta, P.
Melchiorri, A.
Melin, J. -B.
Mendes, L.
Mennella, A.
Mitra, S.
Miville-Deschenes, M. -A.
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Murphy, A.
Naselsky, P.
Natoli, P.
Netterfield, C. B.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
Osborne, S.
Pajot, F.
Pasian, F.
Patanchon, G.
Perdereau, O.
Perotto, L.
Perrotta, F.
Piacentini, F.
Piat, M.
Pierpaoli, E.
Piffaretti, R.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Ponthieu, N.
Poutanen, T.
Pratt, G. W.
Prezeau, G.
Prunet, S.
Puget, J. -L.
Rebolo, R.
Reinecke, M.
Renault, C.
Ricciardi, S.
Riller, T.
Ristorcelli, I.
Rocha, G.
Rosset, C.
Rubino-Martin, J. A.
Rusholme, B.
Sandri, M.
Santos, D.
Schaefer, B. M.
Scott, D.
Seiffert, M. D.
Smoot, G. F.
Starck, J. -L.
Stivoli, F.
Stolyarov, V.
Sunyaev, R.
Sygnet, J. -F.
Tauber, J. A.
Terenzi, L.
Toffolatti, L.
Tomasi, M.
Tristram, M.
Tuovinen, J.
Valenziano, L.
Vibert, L.
Vielva, P.
Villa, F.
Vittorio, N.
Wandelt, B. D.
White, S. D. M.
White, M.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck early results. X. Statistical analysis of Sunyaev-Zeldovich
scaling relations for X-ray galaxy clusters
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: clusters: intracluster medium; X-rays: galaxies: clusters;
cosmology: observations
ID PRE-LAUNCH STATUS; SOUTH-POLE TELESCOPE; SKY SURVEY; PRESSURE PROFILE;
WARPS SURVEY; ROSAT SURVEY; MILKY-WAY; WMAP DATA; CATALOG; SAMPLE
AB All-sky data from the Planck survey and the Meta-Catalogue of X-ray detected Clusters of galaxies (MCXC) are combined to investigate the relationship between the thermal Sunyaev-Zeldovich (SZ) signal and X-ray luminosity. The sample comprises similar to 1600 X-ray clusters with redshifts up to similar to 1 and spans a wide range in X-ray luminosity. The SZ signal is extracted for each object individually, and the statistical significance of the measurement is maximised by averaging the SZ signal in bins of X-ray luminosity, total mass, or redshift. The SZ signal is detected at very high significance over more than two decades in X-ray luminosity (10(43) erg s(-1) less than or similar to L500E(z)(-7/3) less than or similar to 2 x 10(45) erg s(-1)). The relation between intrinsic SZ signal and X-ray luminosity is investigated and the measured SZ signal is compared to values predicted from X-ray data. Planck measurements and X-ray based predictions are found to be in excellent agreement over the whole explored luminosity range. No significant deviation from standard evolution of the scaling relations is detected. For the first time the intrinsic scatter in the scaling relation between SZ signal and X-ray luminosity is measured and found to be consistent with the one in the luminosity - mass relation from X-ray studies. There is no evidence of any deficit in SZ signal strength in Planck data relative to expectations from the X-ray properties of clusters, underlining the robustness and consistency of our overall view of intra-cluster medium properties.
C1 [Arnaud, M.; Piffaretti, R.; Pratt, G. W.; Starck, J. -L.] Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU,Serv Astrophys,CEA,DSM,CNRS, F-91191 Gif Sur Yvette, France.
[Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
[Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Fromenteau, S.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR7164, Paris, France.
[Ashdown, M.; Brown, M. L.; Chon, G.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile.
[Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Dahle, H.] Univ Oslo, Ctr Math Applicat, Oslo, Norway.
[Da Silva, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Challinor, A.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England.
[Melin, J. -B.; Piffaretti, R.; Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France.
[Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Marleau, F.; Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA.
[Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Smoot, G. F.; White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Balbi, A.; Leonardi, R.; Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
[Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
[Flores-Cacho, I.; Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, Tenerife, Spain.
[Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile.
[Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain.
[Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
[Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland.
[Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy.
[Colafrancesco, S.; Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Maino, D.; Tomasi, M.] INAF IASF Milano, Milan, Italy.
[Stivoli, F.] Univ Paris 11, INRIA, Lab Rech Informat, F-91405 Orsay, France.
[Desert, F. -X.] Univ Grenoble 1, IPAG, CNRS, INSU,UMR 5274, F-38041 Grenoble, France.
[Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Chary, R. -R.; Ganga, K.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France.
[Aghanim, N.; Aumont, J.; Douspis, M.; Fromenteau, S.; Lagache, G.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Vibert, L.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, Paris, France.
[Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Dahle, H.; Donzelli, S.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Flores-Cacho, I.; Genova-Santos, R. T.; Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Barreiro, R. B.; Diego, J. M.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Maffei, B.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Ashdown, M.; Brown, M. L.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
[Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France.
[Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France.
[Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, CNRS, IN2P3, Lab Phys Subatom & Cosmol,Inst Natl Polytech Gren, F-38026 Grenoble, France.
[Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, IN2P3, Lab Accelerateur Lineaire, F-91405 Orsay, France.
[Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Banday, A. J.; Bartelmann, M.; Churazov, E.; Dolag, K.; Doerl, U.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Chon, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland.
[Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland.
[Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Mann, R.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Munshi, D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Churazov, E.; Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Bartelmann, M.; Schaefer, B. M.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain.
[Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Piffaretti, R (reprint author), Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU,Serv Astrophys,CEA,DSM,CNRS, Bat 709, F-91191 Gif Sur Yvette, France.
EM rocco.piffaretti@cea.fr
RI Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo,
Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso,
Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi,
Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Piacentini,
Francesco/E-7234-2010; Novikov, Dmitry/P-1807-2015; Stolyarov,
Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Toffolatti,
Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner,
Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon,
Dominique/D-2280-2015; de Gasperis, Giancarlo/C-8534-2012; Gregorio,
Anna/J-1632-2012; Churazov, Eugene/A-7783-2013; Lopez-Caniego,
Marcos/M-4695-2013; Da Silva, Antonio/A-2693-2010; Bartelmann,
Matthias/A-5336-2014; Bouchet, Francois/B-5202-2014; Vielva,
Patricio/F-6745-2014
OI Pierpaoli, Elena/0000-0002-7957-8993; Starck,
Jean-Luc/0000-0003-2177-7794; Zacchei, Andrea/0000-0003-0396-1192;
Hivon, Eric/0000-0003-1880-2733; Polenta, Gianluca/0000-0003-4067-9196;
Sandri, Maura/0000-0003-4806-5375; Cuttaia,
Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099;
Burigana, Carlo/0000-0002-3005-5796; Bouchet,
Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043;
Villa, Fabrizio/0000-0003-1798-861X; Galeotta,
Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379;
Matarrese, Sabino/0000-0002-2573-1243; Pasian,
Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269;
Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840;
Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego,
Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Masi,
Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003;
de Bernardis, Paolo/0000-0001-6547-6446; Forni,
Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412;
Maris, Michele/0000-0001-9442-2754; Franceschi,
Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104;
Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070;
Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio,
Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131;
Piacentini, Francesco/0000-0002-5444-9327; Stolyarov,
Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748;
Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Toffolatti,
Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro,
Rita Belen/0000-0002-6139-4272; de Gasperis,
Giancarlo/0000-0003-2899-2171; Da Silva, Antonio/0000-0002-6385-1609;
Vielva, Patricio/0000-0003-0051-272X
FU Centre National d'Etudes Spatiales (CNES); ESA; CNES;
CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA);
STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC (Finland);
DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO
(Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA
(EU)
FX This research has made use of the X-Rays Clusters Database (BAX) which
is operated by the Laboratoire d'Astrophysique de Tarbes-Toulouse
(LATT), under contract with the Centre National d'Etudes Spatiales
(CNES). We acknowledge the use of the HEALPix package (Gorski et al.
2005). The Planck Collaboration acknowledges the support of: ESA; CNES
and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and
DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF
and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space
(Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES
(Portugal); and DEISA (EU). A description of the Planck Collaboration
and a list of its members, indicating which technical or scientific
activities they have been involved in, can be found at
http://www.rssd.esa.int/Planck.
NR 88
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FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD DEC
PY 2011
VL 536
AR A10
DI 10.1051/0004-6361/201116457
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100011
ER
PT J
AU Eiroa, C
Marshall, JP
Mora, A
Krivov, AV
Montesinos, B
Absil, O
Ardila, D
Arevalo, M
Augereau, JC
Bayo, A
Danchi, W
del Burgo, C
Ertel, S
Fridlund, M
Gonzalez-Garcia, BM
Heras, AM
Lebreton, J
Liseau, R
Maldonado, J
Meeus, G
Montes, D
Pilbratt, GL
Roberge, A
Sanz-Forcada, J
Stapelfeldt, K
Thebault, P
White, GJ
Wolf, S
AF Eiroa, C.
Marshall, J. P.
Mora, A.
Krivov, A. V.
Montesinos, B.
Absil, O.
Ardila, D.
Arevalo, M.
Augereau, J. -Ch
Bayo, A.
Danchi, W.
del Burgo, C.
Ertel, S.
Fridlund, M.
Gonzalez-Garcia, B. M.
Heras, A. M.
Lebreton, J.
Liseau, R.
Maldonado, J.
Meeus, G.
Montes, D.
Pilbratt, G. L.
Roberge, A.
Sanz-Forcada, J.
Stapelfeldt, K.
Thebault, P.
White, G. J.
Wolf, S.
TI Herschel discovery of a new class of cold, faint debris discs
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; planetary systems; stars: individual: alpha Men
(HIP 29271); stars: individual: HD 88230 (HIP 49908); stars: individual:
HD 210277 (HIP 109378)
ID MAIN-SEQUENCE STARS; DISKS; PLANETS; IMAGES; PACS
AB We present Herschel PACS 100 and 160 mu m observations of the solar-type stars alpha Men, HD 88230 and HD 210277, which form part of the FGK stars sample of the Herschel open time key programme (OTKP) DUNES (DUst around NEarby S tars). Our observations show small infrared excesses at 160 mu m for all three stars. HD 210277 also shows a small excess at 100 mu m, while the 100 mu m fluxes of alpha Men and HD 88230 agree with the stellar photospheric predictions. We attribute these infrared excesses to a new class of cold, faint debris discs. Both alpha Men and HD 88230 are spatially resolved in the PACS 160 mu m images, while HD 210277 is point-like at that wavelength. The projected linear sizes of the extended emission lie in the range from similar to 115 to <= 250 AU. The estimated black body temperatures from the 100 and 160 mu m fluxes are less than or similar to 22 K, and the fractional luminosity of the cold dust is L-dust/L-* similar to 10(-6), close to the luminosity of the solar-system's Kuiper belt. These debris discs are the coldest and faintest discs discovered so far around mature stars, so they cannot be explained easily invoking "classical" debris disc models.
C1 [Eiroa, C.; Marshall, J. P.; Maldonado, J.; Meeus, G.] Univ Autonoma Madrid, Fac Ciencias, Dpt Fis Teor, E-28049 Madrid, Spain.
[Mora, A.] ESA ESAC Gaia SOC, Madrid, Spain.
[Krivov, A. V.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany.
[Krivov, A. V.] Univ Jena, Univ Sternwarte, D-07745 Jena, Germany.
[Montesinos, B.; Arevalo, M.; Sanz-Forcada, J.] Ctr Astrobiol INTA CSIC, Dpt Astrofis, Madrid, Spain.
[Absil, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium.
[Ardila, D.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Augereau, J. -Ch; Lebreton, J.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France.
[Bayo, A.] European Space Observ, Santiago 19, Chile.
[Danchi, W.; Roberge, A.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[del Burgo, C.] UNINOVA CA3, P-2825149 Monte De Caparica, Caparica, Portugal.
[Ertel, S.; Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany.
[Fridlund, M.; Heras, A. 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, Spain.
[Liseau, R.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden.
[Montes, D.] Univ Complutense Madrid, Fac Ciencias Fis, Dpt Astrofis, E-28040 Madrid, Spain.
[Stapelfeldt, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[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, Chilton OX11 0QX, England.
RP Eiroa, C (reprint author), Univ Autonoma Madrid, Fac Ciencias, Dpt Fis Teor, E-28049 Madrid, Spain.
EM carlos.eiroa@uam.es
RI Roberge, Aki/D-2782-2012; Stapelfeldt, Karl/D-2721-2012; Montes,
David/B-9329-2014; Sanz-Forcada, Jorge/C-3176-2017; Montesinos,
Benjamin/C-3493-2017
OI Marshall, Jonathan/0000-0001-6208-1801; Roberge,
Aki/0000-0002-2989-3725; Montes, David/0000-0002-7779-238X;
Sanz-Forcada, Jorge/0000-0002-1600-7835; Montesinos,
Benjamin/0000-0002-7982-2095
NR 26
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD DEC
PY 2011
VL 536
AR L4
DI 10.1051/0004-6361/201117797
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100031
ER
PT J
AU Giustini, M
Cappi, M
Chartas, G
Dadina, M
Eracleous, M
Ponti, G
Proga, D
Tombesi, F
Vignali, C
Palumbo, GGC
AF Giustini, M.
Cappi, M.
Chartas, G.
Dadina, M.
Eracleous, M.
Ponti, G.
Proga, D.
Tombesi, F.
Vignali, C.
Palumbo, G. G. C.
TI Variable X-ray absorption in the mini-BAL QSO PG 1126-041
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: spectroscopic; techniques: photometric; accretion, accretion
disks; methods: data analysis; quasars: individual: PG 1126-041; X-rays:
individuals: PG 1126-041
ID ACTIVE GALACTIC NUCLEI; BRIGHT QUASAR SURVEY; CONTINUUM
ENERGY-DISTRIBUTIONS; EMISSION-LINE PROPERTIES; HIGH-VELOCITY OUTFLOWS;
DRIVEN DISK WINDS; XMM-NEWTON; STELLAR OBJECTS; DATA RELEASE;
BLACK-HOLES
AB Context. X-ray studies of active galactic nuclei (AGN) with powerful nuclear winds are important for constraining the physics of the inner accretion/ejection flow around supermassive black holes (SMBHs) and for understanding the impact of such winds on the AGN environment.
Aims. Our main scientific goal is to constrain the properties of the circum-nuclear matter close to the SMBH in the mini-broad absorption line quasar (mini-BAL QSO) PG 1126-041 using a multi-epoch observational campaign with XMM-Newton.
Methods. We performed temporally resolved X-ray spectroscopy and simultaneous UV and X-ray photometry on the most complete set of observations and on the deepest X-ray exposure of a mini-BAL QSO ever.
Results. We found complex X-ray spectral variability on time scales of both months and hours, which is best reproduced by means of variable massive ionized absorbers along the line of sight. As a consequence, the observed optical-to-X-ray spectral index is found to be variable with time. In the highest signal-to-noise observation we detected highly ionized X-ray absorbing material outflowing much faster (upsilon(X) similar to 16 500 km s(-1)) than the UV absorbing one (upsilon(uv) similar to 5000 km s(-1)). This highly ionized absorber is found to be variable on very short (a few kiloseconds) time scales.
Conclusions. Our findings are qualitatively consistent with line-driven accretion disk winds scenarios. Our observations have opened the time-resolved X-ray spectral analysis field for mini-BAL QSOs. Only with future deep studies will we be able to map the dynamics of the inner flow and understand the physics of AGN winds and their impact on the environment.
C1 [Giustini, M.; Vignali, C.; Palumbo, G. G. C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Giustini, M.; Cappi, M.; Dadina, M.] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy.
[Giustini, M.; Eracleous, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA USA.
[Chartas, G.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Eracleous, M.] Penn State Univ, Ctr Gravitat Wave Phys, University Pk, PA 16802 USA.
[Ponti, G.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Giustini, M.; Proga, D.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Tombesi, F.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Vignali, C.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
RP Giustini, M (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy.
EM giustini@iasfbo.inaf.it
RI Vignali, Cristian/J-4974-2012; Cappi, Massimo/F-4813-2015;
OI Vignali, Cristian/0000-0002-8853-9611; Cappi,
Massimo/0000-0001-6966-8920; Dadina, Mauro/0000-0002-7858-7564
FU ESA Member States; NASA [NNXlOAEllG, NAS 8-39073]; ASI/INAF [I/088/06/0,
I/009/10/0]; Chandra award [TM0-11010X]; National Science Fundation
[AST-0807993]; EU [FP7-PEOPLE-2009-IEF-254279]
FX Based on observations obtained with XMM-Newton, an ESA science mission
with instruments and contributions directly funded by ESA Member States
and NASA.; M.G., M. C., M. D., and C. V. acknowledge financial support
from the ASI/INAF contracts I/088/06/0 and I/009/10/0. G. C. and M. G.
acknowledge support provided by NASA grant NNXlOAEllG. D. P. and M. G.
acknowledge support provided by the Chandra award TM0-11010X issued by
the Chandra X-ray Observatory Center, which is operated by the
Smithsonian Astrophysical Observatory for and on behalf of NASA under
contract NAS 8-39073. M. E. acknowledges support from the National
Science Fundation under grant AST-0807993. G. P. acknowledges support
via an EU Marie Curie Intra-European Fellowship under contract No.
FP7-PEOPLE-2009-IEF-254279. We thank the referee for the thoughtful
comments that helped improve the article presentation. 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 88
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FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD DEC
PY 2011
VL 536
DI 10.1051/0004-6361/201117732
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100058
ER
PT J
AU Klochkov, D
Ferrigno, C
Santangelo, A
Staubert, R
Kretschmar, P
Caballero, I
Postnov, K
Wilson-Hodge, CA
AF Klochkov, D.
Ferrigno, C.
Santangelo, A.
Staubert, R.
Kretschmar, P.
Caballero, I.
Postnov, K.
Wilson-Hodge, C. A.
TI Quasi-periodic flares in EXO2030+375 observed with INTEGRAL
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: neutron; accretion, accretion disks; X-rays: binaries
ID X-RAY PULSAR; EXO 2030+375; NEUTRON-STAR; VELA X-1; LMC X-4;
EXO-2030+375; OUTBURST; ACCRETION; EVOLUTION; VARIABILITY
AB Context. Episodic flaring activity is a common feature of X-ray pulsars in HMXBs. In some Be/X-ray binaries flares were observed in quiescence or prior to outbursts. EXO2030+375 is a Be/X-ray binary showing "normal" outbursts almost every similar to 46 days, near periastron passage of the orbital revolution. Some of these outbursts were occasionally monitored with the INTEGRAL observatory.
Aims. The INTEGRAL data revealed strong quasi-periodic flaring activity during the rising part of one of the system's outburst. Such activity has previously been observed in EXO2030+375 only once, in 1985 with EXOSAT. (Some indications of single flares have also been observed with other satellites.)
Methods. We present the analysis of the flaring behavior of the source based on INTEGRAL data and compare it with the flares observed in EXO2030+375 in 1985.
Results. Based on the observational properties of the flares, we argue that the instability at the inner edge of the accretion disk is the most probable cause of the flaring activity.
C1 [Klochkov, D.; Santangelo, A.; Staubert, R.] Univ Tubingen IAAT, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Ferrigno, C.] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
[Kretschmar, P.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, Villanueva De La Canada, Madrid, Spain.
[Caballero, I.] Univ Paris Diderot, CNRS, CEA Saclay, DSM,IRFU,SAp,UMR AIM 7158,CEA, F-91191 Gif Sur Yvette, France.
[Postnov, K.] Moscow M V Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Wilson-Hodge, C. A.] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Klochkov, D (reprint author), Univ Tubingen IAAT, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM klochkov@astro.uni-tuebingen.de
RI Ferrigno, Carlo/H-4139-2012;
OI Kretschmar, Peter/0000-0001-9840-2048
FU Carl-Zeiss-Stiftung; DLR [BA5027]; ESA member states
FX The work was supported by the Carl-Zeiss-Stiftung and by DLR grant
BA5027. This research is based on observations with INTEGRAL, an ESA
project with instruments and science data centre funded by ESA member
states. The authors thank the anonymous referee for useful suggestions.
NR 35
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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 DEC
PY 2011
VL 536
AR L8
DI 10.1051/0004-6361/201118185
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100035
ER
PT J
AU Mennella, A
Bersanelli, M
Butler, RC
Curto, A
Cuttaia, F
Davis, RJ
Dick, J
Frailis, M
Galeotta, S
Gregorio, A
Kurki-Suonio, H
Lawrence, CR
Leach, S
Leahy, JP
Lowe, S
Maino, D
Mandolesi, N
Maris, M
Martinez-Gonzalez, E
Meinhold, PR
Morgante, G
Pearson, D
Perrotta, F
Polenta, G
Poutanen, T
Sandri, M
Seiffert, MD
Suur-Uski, AS
Tavagnacco, D
Terenzi, L
Tomasi, M
Valiviita, J
Villa, F
Watson, R
Wilkinson, A
Zacchei, A
Zonca, A
Aja, B
Artal, E
Baccigalupi, C
Banday, AJ
Barreiro, RB
Bartlett, JG
Bartolo, N
Battaglia, P
Bennett, K
Bonaldi, A
Bonavera, L
Borrill, J
Bouchet, FR
Burigana, C
Cabella, P
Cappellini, B
Chen, X
Colombo, L
Cruz, M
Danese, L
D'Arcangelo, O
Davies, RD
de Gasperis, G
de Rosa, A
de Zotti, G
Dickinson, C
Diego, JM
Donzelli, S
Efstathiou, G
Ensslin, TA
Eriksen, HK
Falvella, MC
Finelli, F
Foley, S
Franceschet, C
Franceschi, E
Gaier, TC
Genova-Santos, RT
George, D
Gomez, F
Gonzalez-Nuevo, J
Gorski, KM
Gruppuso, A
Hansen, FK
Herranz, D
Herreros, JM
Hoyland, RJ
Hughes, N
Jewell, J
Jukkala, P
Juvela, M
Kangaslahti, P
Keihanen, E
Keskitalo, R
Kilpia, VH
Kisner, TS
Knoche, J
Knox, L
Laaninen, M
Lahteenmaki, A
Lamarre, JM
Leonardi, R
Leon-Tavares, J
Leutenegger, P
Lilje, PB
Lopez-Caniego, M
Lubin, PM
Malaspina, M
Marinucci, D
Massardi, M
Matarrese, S
Matthai, F
Melchiorri, A
Mendes, L
Miccolis, M
Migliaccio, M
Mitra, S
Moss, A
Natoli, P
Nesti, R
Norgaard-Nielsen, HU
Pagano, L
Paladini, R
Paoletti, D
Partridge, B
Pasian, F
Pettorino, V
Pietrobon, D
Pospieszalski, M
Prezeau, G
Prina, M
Procopio, P
Puget, JL
Quercellini, C
Rachen, JP
Rebolo, R
Reinecke, M
Ricciardi, S
Robbers, G
Rocha, G
Roddis, N
Rubino-Martin, JA
Savelainen, M
Scott, D
Silvestri, R
Simonetto, A
Sjoman, P
Smoot, GF
Sozzi, C
Stringhetti, L
Tauber, JA
Tofani, G
Toffolatti, L
Tuovinen, J
Turler, M
Umana, G
Valenziano, L
Varis, J
Vielva, P
Vittorio, N
Wade, LA
Watson, C
White, SDM
Winder, F
AF Mennella, A.
Bersanelli, M.
Butler, R. C.
Curto, A.
Cuttaia, F.
Davis, R. J.
Dick, J.
Frailis, M.
Galeotta, S.
Gregorio, A.
Kurki-Suonio, H.
Lawrence, C. R.
Leach, S.
Leahy, J. P.
Lowe, S.
Maino, D.
Mandolesi, N.
Maris, M.
Martinez-Gonzalez, E.
Meinhold, P. R.
Morgante, G.
Pearson, D.
Perrotta, F.
Polenta, G.
Poutanen, T.
Sandri, M.
Seiffert, M. D.
Suur-Uski, A. -S.
Tavagnacco, D.
Terenzi, L.
Tomasi, M.
Valiviita, J.
Villa, F.
Watson, R.
Wilkinson, A.
Zacchei, A.
Zonca, A.
Aja, B.
Artal, E.
Baccigalupi, C.
Banday, A. J.
Barreiro, R. B.
Bartlett, J. G.
Bartolo, N.
Battaglia, P.
Bennett, K.
Bonaldi, A.
Bonavera, L.
Borrill, J.
Bouchet, F. R.
Burigana, C.
Cabella, P.
Cappellini, B.
Chen, X.
Colombo, L.
Cruz, M.
Danese, L.
D'Arcangelo, O.
Davies, R. D.
de Gasperis, G.
de Rosa, A.
de Zotti, G.
Dickinson, C.
Diego, J. M.
Donzelli, S.
Efstathiou, G.
Ensslin, T. A.
Eriksen, H. K.
Falvella, M. C.
Finelli, F.
Foley, S.
Franceschet, C.
Franceschi, E.
Gaier, T. C.
Genova-Santos, R. T.
George, D.
Gomez, F.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gruppuso, A.
Hansen, F. K.
Herranz, D.
Herreros, J. M.
Hoyland, R. J.
Hughes, N.
Jewell, J.
Jukkala, P.
Juvela, M.
Kangaslahti, P.
Keihanen, E.
Keskitalo, R.
Kilpia, V. -H.
Kisner, T. S.
Knoche, J.
Knox, L.
Laaninen, M.
Lahteenmaki, A.
Lamarre, J. -M.
Leonardi, R.
Leon-Tavares, J.
Leutenegger, P.
Lilje, P. B.
Lopez-Caniego, M.
Lubin, P. M.
Malaspina, M.
Marinucci, D.
Massardi, M.
Matarrese, S.
Matthai, F.
Melchiorri, A.
Mendes, L.
Miccolis, M.
Migliaccio, M.
Mitra, S.
Moss, A.
Natoli, P.
Nesti, R.
Norgaard-Nielsen, H. U.
Pagano, L.
Paladini, R.
Paoletti, D.
Partridge, B.
Pasian, F.
Pettorino, V.
Pietrobon, D.
Pospieszalski, M.
Prezeau, G.
Prina, M.
Procopio, P.
Puget, J. -L.
Quercellini, C.
Rachen, J. P.
Rebolo, R.
Reinecke, M.
Ricciardi, S.
Robbers, G.
Rocha, G.
Roddis, N.
Rubino-Martin, J. A.
Savelainen, M.
Scott, D.
Silvestri, R.
Simonetto, A.
Sjoman, P.
Smoot, G. F.
Sozzi, C.
Stringhetti, L.
Tauber, J. A.
Tofani, G.
Toffolatti, L.
Tuovinen, J.
Tuerler, M.
Umana, G.
Valenziano, L.
Varis, J.
Vielva, P.
Vittorio, N.
Wade, L. A.
Watson, C.
White, S. D. M.
Winder, F.
TI Planck early results. III. First assessment of the Low Frequency
Instrument in-flight performance
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmic background radiation; cosmology: observations; space vehicles:
instruments; instrumentation: detectors
ID MAP-MAKING ALGORITHM; SKY MAPS; DESTRIPING TECHNIQUE; RADIOMETERS;
POLARIZATION; CALIBRATION; MADAM
AB The scientific performance of the Planck Low Frequency Instrument (LFI) after one year of in-orbit operation is presented. We describe the main optical parameters and discuss photometric calibration, white noise sensitivity, and noise properties. A preliminary evaluation of the impact of the main systematic effects is presented. For each of the performance parameters, we outline the methods used to obtain them from the flight data and provide a comparison with pre-launch ground assessments, which are essentially confirmed in flight.
C1 [Mennella, A.; Bersanelli, M.; Maino, D.; Tomasi, M.; Franceschet, C.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Poutanen, T.; Lahteenmaki, A.; Leon-Tavares, J.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Polenta, G.; Natoli, P.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
[Falvella, M. C.] Agenzia Spaziale Italiana, Rome, Italy.
[Bartlett, J. G.; Smoot, G. F.] Univ Paris 07, CNRS, UMR7164, Paris, France.
[Bonavera, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Banday, A. J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway.
[Hughes, N.; Jukkala, P.; Kilpia, V. -H.; Sjoman, P.] DA Design Oy, Jokioinen, Finland.
[Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Aja, B.; Artal, E.] Univ Cantabria, Dept Ingn Comunicac, E-39005 Santander, Spain.
[Cruz, M.] Univ Cantabria, Dept Matemat Estadist & Computac, E-39005 Santander, Spain.
[Moss, A.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Colombo, L.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA.
[Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Juvela, M.; Keihanen, E.; Keskitalo, R.; Savelainen, M.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Meinhold, P. R.; Zonca, A.; Leonardi, R.; Lubin, P. M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Bartolo, N.; Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Melchiorri, A.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Gregorio, A.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Cabella, P.; de Gasperis, G.; Migliaccio, M.; Quercellini, C.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Marinucci, D.] Univ Roma Tor Vergata, Dipartimento Matemat, I-00173 Rome, Italy.
[Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain.
[Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain.
[Foley, S.; Watson, C.] European Space Agcy, ESOC, Darmstadt, Germany.
[Bennett, K.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
[Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA.
[Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Lahteenmaki, A.; Savelainen, M.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland.
[Nesti, R.; Tofani, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy.
[Bonaldi, A.; de Zotti, G.; Massardi, M.] Osserv Astron Padova, INAF, Padua, Italy.
[Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Mennella, A.; Frailis, M.; Galeotta, S.; Maris, M.; Tavagnacco, D.; Zacchei, A.; Pasian, F.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Butler, R. C.; Cuttaia, F.; Mandolesi, N.; Morgante, G.; Sandri, M.; Terenzi, L.; Villa, F.; Burigana, C.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Malaspina, M.; Natoli, P.; Paoletti, D.; Procopio, P.; Ricciardi, S.; Stringhetti, L.; Valenziano, L.] INAF IASF Bologna, Bologna, Italy.
[Bersanelli, M.; Maino, D.; Tomasi, M.; Cappellini, B.; Donzelli, S.] INAF IASF Milano, Milan, Italy.
[Tuerler, M.] Univ Geneva, ISDC Data Ctr Astrophys, Versoix, Switzerland.
[Chen, X.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Puget, J. -L.] Univ Paris 11, CNRS, UMR 8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Bouchet, F. R.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, Paris, France.
[Efstathiou, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Valiviita, J.; Donzelli, S.; Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Genova-Santos, R. T.; Gomez, F.; Herreros, J. M.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Curto, A.; Martinez-Gonzalez, E.; Barreiro, R. B.; Diego, J. M.; Herranz, D.; Lopez-Caniego, M.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[D'Arcangelo, O.; Simonetto, A.; Sozzi, C.] CNR ENEA EURATOM Assoc, Ist Fis Plasma, Milan, Italy.
[Lawrence, C. R.; Pearson, D.; Seiffert, M. D.; Bartlett, J. G.; Colombo, L.; Gaier, T. C.; Gorski, K. M.; Jewell, J.; Kangaslahti, P.; Keskitalo, R.; Mitra, S.; Pagano, L.; Pietrobon, D.; Prezeau, G.; Prina, M.; Rocha, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Davis, R. J.; Leahy, J. P.; Lowe, S.; Watson, R.; Wilkinson, A.; Davies, R. D.; Dickinson, C.; Roddis, N.; Winder, F.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
[Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Banday, A. J.; Ensslin, T. A.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Robbers, G.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland.
[Pospieszalski, M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Laaninen, M.] Nokia Electr Ltd, Helsinki, Finland.
[Dick, J.; Leach, S.; Perrotta, F.; Baccigalupi, C.; Bonavera, L.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Pettorino, V.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[George, D.] Univ Manchester, Sch Elect & Elect Engn, Manchester M13 9PL, Lancs, England.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA.
[Battaglia, P.; Leutenegger, P.; Miccolis, M.; Silvestri, R.] Thales Alenia Space Italia SpA, I-20090 Vimodrone, MI, Italy.
[Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Mennella, A (reprint author), Univ Milan, Dipartimento Fis, Via Celoria 16, Milan, Italy.
EM aniello.mennella@fisica.unimi.it
RI Butler, Reginald/N-4647-2015; Artal, Eduardo/H-5546-2015;
Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015;
Valiviita, Jussi/A-9058-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi,
Maurizio/I-1234-2016; Colombo, Loris/J-2415-2016; Aja,
Beatriz/H-5573-2015; bonavera, laura/E-9368-2017; Lilje,
Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012; Cruz,
Marcos/N-3429-2014; Barreiro, Rita Belen/N-5442-2014; Martinez-Gonzalez,
Enrique/E-9534-2015; Sozzi, Carlo/F-4158-2012; Gregorio,
Anna/J-1632-2012; Lopez-Caniego, Marcos/M-4695-2013; Bouchet,
Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva,
Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz,
Diego/K-9143-2014
OI Galeotta, Samuele/0000-0002-3748-5115; TERENZI,
LUCA/0000-0001-9915-6379; Watson, Robert/0000-0002-5873-0124; Zacchei,
Andrea/0000-0003-0396-1192; Lilje, Per/0000-0003-4324-7794; Paoletti,
Daniela/0000-0003-4761-6147; Polenta, Gianluca/0000-0003-4067-9196;
Sandri, Maura/0000-0003-4806-5375; Cuttaia,
Francesco/0000-0001-6608-5017; Burigana, Carlo/0000-0002-3005-5796;
Bouchet, Francois/0000-0002-8051-2924; Ricciardi,
Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X;
Matarrese, Sabino/0000-0002-2573-1243; Lowe, Stuart/0000-0002-2975-9032;
Pasian, Fabio/0000-0002-4869-3227; Finelli, Fabio/0000-0002-6694-3269;
Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840;
Frailis, Marco/0000-0002-7400-2135; Nesti, Renzo/0000-0003-0303-839X;
Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio,
Anna/0000-0003-4028-8785; Butler, Reginald/0000-0003-4366-5996;
Stringhetti, Luca/0000-0002-3961-9068; Melchiorri,
Alessandro/0000-0001-5326-6003; Zonca, Andrea/0000-0001-6841-1058;
Morgante, Gianluca/0000-0001-9234-7412; Maris,
Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591;
Valenziano, Luca/0000-0002-1170-0104; Artal,
Eduardo/0000-0002-2569-1894; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292;
Valiviita, Jussi/0000-0001-6225-3693; Kurki-Suonio,
Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131;
Colombo, Loris/0000-0003-4572-7732; Aja, Beatriz/0000-0002-4229-2334;
bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose
Alberto/0000-0001-5289-3021; de Gasperis, Giancarlo/0000-0003-2899-2171;
Cruz, Marcos/0000-0002-4767-530X; Barreiro, Rita
Belen/0000-0002-6139-4272; Martinez-Gonzalez,
Enrique/0000-0002-0179-8590; Sozzi, Carlo/0000-0001-8951-0071; Vielva,
Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386;
Herranz, Diego/0000-0003-4540-1417
FU ESA; NASA (USA); CNES; CNRS/INSU-IN2P3; ASI; Finnish Funding Agency for
Technology and Innovation (Tekes); Academy of Finland; CSC; DEISA (EU)
FX Planck (http://www.esa.int/Planck) is a project of the European Space
Agency (ESA) with instruments provided by two scientific consortia
funded by ESA member states (in particular the lead countries France and
Italy), with contributions from NASA (USA) and telescope reflectors
provided by a collaboration between ESA and a scientific consortium led
and funded by Denmark.; Planck is too large a project to allow full
acknowledgement of all contributions by individuals, institutions,
industries, and funding agencies. The main entities involved in the
mission operations are as follows. The European Space Agency operates
the satellite via its Mission Operations Centre located at ESOC
(Darmstadt, Germany) and coordinates scientific operations via the
Planck Science Office located at ESAC (Madrid, Spain). Two Consortia,
comprising around 50 scientific institutes within Europe, the USA, and
Canada, and funded by agencies from the participating countries,
developed the scientific instruments LFI and HFI, and continue to
operate them via Instrument Operations Teams located in Trieste (Italy)
and Orsay (France). The Consortia are also responsible for scientific
processing of the acquired data. The Consortia are led by the Principal
Investigators: J.-L. Puget in France for HFI (funded principally by CNES
and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded
principally via ASI). NASA's US Planck Project, based at JPL and
involving scientists at many US institutions, contributes significantly
to the efforts of these two Consortia. In Finland, the Planck LFI 70 GHz
work was supported by the Finnish Funding Agency for Technology and
Innovation (Tekes). This work was also supported by the Academy of
Finland, CSC, and DEISA (EU).
NR 61
TC 105
Z9 105
U1 2
U2 12
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 DEC
PY 2011
VL 536
AR A3
DI 10.1051/0004-6361/201116480
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100004
ER
PT J
AU Zacchei, A
Maino, D
Baccigalupi, C
Bersanelli, M
Bonaldi, A
Bonavera, L
Burigana, C
Butler, RC
Cuttaia, F
de Zotti, G
Dick, J
Frailis, M
Galeotta, S
Gonzalez-Nuevo, J
Gorski, KM
Gregorio, A
Keihanen, E
Keskitalo, R
Knoche, J
Kurki-Suonio, H
Lawrence, CR
Leach, S
Leahy, JP
Lopez-Caniego, M
Mandolesi, N
Maris, M
Matthai, F
Meinhold, PR
Mennella, A
Morgante, G
Morisset, N
Natoli, P
Pasian, F
Perrotta, F
Polenta, G
Poutanen, T
Reinecke, M
Ricciardi, S
Rohlfs, R
Sandri, M
Suur-Uski, AS
Tauber, JA
Tavagnacco, D
Terenzi, L
Tomasi, M
Valiviita, J
Villa, F
Zonca, A
Banday, AJ
Barreiro, RB
Bartlett, JG
Bartolo, N
Bedini, L
Bennett, K
Binko, P
Borrill, J
Bouchet, FR
Bremer, M
Cabella, P
Cappellini, B
Chen, X
Colombo, L
Cruz, M
Curto, A
Danese, L
Davies, RD
Davis, RJ
de Gasperis, G
de Rosa, A
de Troia, G
Dickinson, C
Diego, JM
Donzelli, S
Dorl, U
Efstathiou, G
Ensslin, TA
Eriksen, HK
Falvella, MC
Finelli, F
Franceschi, E
Gaier, TC
Gasparo, F
Genova-Santos, RT
Giardino, G
Gomez, F
Gruppuso, A
Hansen, FK
Hell, R
Herranz, D
Hovest, W
Huynh, M
Jewell, J
Juvela, M
Kisner, TS
Knox, L
Lahteenmaki, A
Lamarre, JM
Leonardi, R
Leon-Tavares, J
Lilje, PB
Lubin, PM
Maggio, G
Marinucci, D
Martinez-Gonzalez, E
Massardi, M
Matarrese, S
Meharga, MT
Melchiorri, A
Migliaccio, M
Mitra, S
Moss, A
Norgaard-Nielsen, HU
Pagano, L
Paladini, R
Paoletti, D
Partridge, B
Pearson, D
Pettorino, V
Pietrobon, D
Prezeau, G
Procopio, P
Puget, JL
Quercellini, C
Rachen, JP
Rebolo, R
Robbers, G
Rocha, G
Rubino-Martin, JA
Salerno, E
Savelainen, M
Scott, D
Seiffert, MD
Silk, JI
Smoot, GF
Sternberg, J
Stivoli, F
Stompor, R
Tofani, G
Toffolatti, L
Tuovinen, J
Turler, M
Umana, G
Vielva, P
Vittorio, N
Vuerli, C
Wade, LA
Watson, R
White, SDM
Wilkinson, A
AF Zacchei, A.
Maino, D.
Baccigalupi, C.
Bersanelli, M.
Bonaldi, A.
Bonavera, L.
Burigana, C.
Butler, R. C.
Cuttaia, F.
de Zotti, G.
Dick, J.
Frailis, M.
Galeotta, S.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gregorio, A.
Keihanen, E.
Keskitalo, R.
Knoche, J.
Kurki-Suonio, H.
Lawrence, C. R.
Leach, S.
Leahy, J. P.
Lopez-Caniego, M.
Mandolesi, N.
Maris, M.
Matthai, F.
Meinhold, P. R.
Mennella, A.
Morgante, G.
Morisset, N.
Natoli, P.
Pasian, F.
Perrotta, F.
Polenta, G.
Poutanen, T.
Reinecke, M.
Ricciardi, S.
Rohlfs, R.
Sandri, M.
Suur-Uski, A. -S.
Tauber, J. A.
Tavagnacco, D.
Terenzi, L.
Tomasi, M.
Valiviita, J.
Villa, F.
Zonca, A.
Banday, A. J.
Barreiro, R. B.
Bartlett, J. G.
Bartolo, N.
Bedini, L.
Bennett, K.
Binko, P.
Borrill, J.
Bouchet, F. R.
Bremer, M.
Cabella, P.
Cappellini, B.
Chen, X.
Colombo, L.
Cruz, M.
Curto, A.
Danese, L.
Davies, R. D.
Davis, R. J.
de Gasperis, G.
de Rosa, A.
de Troia, G.
Dickinson, C.
Diego, J. M.
Donzelli, S.
Doerl, U.
Efstathiou, G.
Ensslin, T. A.
Eriksen, H. K.
Falvella, M. C.
Finelli, F.
Franceschi, E.
Gaier, T. C.
Gasparo, F.
Genova-Santos, R. T.
Giardino, G.
Gomez, F.
Gruppuso, A.
Hansen, F. K.
Hell, R.
Herranz, D.
Hovest, W.
Huynh, M.
Jewell, J.
Juvela, M.
Kisner, T. S.
Knox, L.
Lahteenmaki, A.
Lamarre, J. -M.
Leonardi, R.
Leon-Tavares, J.
Lilje, P. B.
Lubin, P. M.
Maggio, G.
Marinucci, D.
Martinez-Gonzalez, E.
Massardi, M.
Matarrese, S.
Meharga, M. T.
Melchiorri, A.
Migliaccio, M.
Mitra, S.
Moss, A.
Norgaard-Nielsen, H. U.
Pagano, L.
Paladini, R.
Paoletti, D.
Partridge, B.
Pearson, D.
Pettorino, V.
Pietrobon, D.
Prezeau, G.
Procopio, P.
Puget, J. -L.
Quercellini, C.
Rachen, J. P.
Rebolo, R.
Robbers, G.
Rocha, G.
Rubino-Martin, J. A.
Salerno, E.
Savelainen, M.
Scott, D.
Seiffert, M. D.
Silk, J. I.
Smoot, G. F.
Sternberg, J.
Stivoli, F.
Stompor, R.
Tofani, G.
Toffolatti, L.
Tuovinen, J.
Tuerler, M.
Umana, G.
Vielva, P.
Vittorio, N.
Vuerli, C.
Wade, L. A.
Watson, R.
White, S. D. M.
Wilkinson, A.
TI Planck early results. V. The Low Frequency Instrument data processing
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: data analysis; cosmic background radiation; cosmology:
observations; surveys
ID PRE-LAUNCH STATUS; MAP-MAKING ALGORITHM; 30 GHZ DATA; MISSION; LFI;
CALIBRATION; NOISE; MADAM
AB We describe the processing of data from the Low Frequency Instrument (LFI) used in production of the Planck Early Release Compact Source Catalogue (ERCSC). In particular, we discuss the steps involved in reducing the data from telemetry packets to cleaned, calibrated, time-ordered data (TOD) and frequency maps. Data are continuously calibrated using the modulation of the temperature of the cosmic microwave background radiation induced by the motion of the spacecraft. Noise properties are estimated from TOD from which the sky signal has been removed using a generalized least square map-making algorithm. Measured 1/f noise knee-frequencies range from similar to 100 mHz at 30 GHz to a few tens of mHz at 70 GHz. A destriping code (Madam) is employed to combine radiometric data and pointing information into sky maps, minimizing the variance of correlated noise. Noise covariance matrices required to compute statistical uncertainties on LFI and Planck products are also produced. Main beams are estimated down to the approximate to-10 dB level using Jupiter transits, which are also used for geometrical calibration of the focal plane.
C1 [Zacchei, A.; Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Tavagnacco, D.; Gasparo, F.; Maggio, G.; Vuerli, C.] INAF Osservatorio Astron Trieste, Trieste, Italy.
[Poutanen, T.; Lahteenmaki, A.; Leon-Tavares, J.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
[Falvella, M. C.] Agenzia Spaziale Italiana, Rome, Italy.
[Bartlett, J. G.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France.
[Bonavera, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Bedini, L.; Salerno, E.] CNR ISTI, Area Ric, Pisa, Italy.
[Banday, A. J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway.
[Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Cruz, M.] Univ Cantabria, Dept Matemat Estadist & Computac, E-39005 Santander, Spain.
[Moss, A.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Colombo, L.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA.
[Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Juvela, M.; Savelainen, M.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Meinhold, P. R.; Zonca, A.; Leonardi, R.; Lubin, P. M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Silk, J. I.] Univ Oxford, Dept Phys, Oxford, England.
[Bartolo, N.; Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Melchiorri, A.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Maino, D.; Bersanelli, M.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy.
[Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Cabella, P.; de Gasperis, G.; de Troia, G.; Migliaccio, M.; Quercellini, C.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, Rome, Italy.
[Marinucci, D.] Univ Roma Tor Vergata, Dipartimento Matemat, Rome, Italy.
[Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain.
[Leonardi, R.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain.
[Tauber, J. A.; Bennett, K.; Bremer, M.; Giardino, G.; Leonardi, R.; Sternberg, J.] European Space Agcy, ESTEC, NL-2201 AZ Noordwijk, Netherlands.
[Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA.
[Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Lahteenmaki, A.; Savelainen, M.] Univ Helsinki, Helsinki, Finland.
[Tofani, G.] INAF Osservatorio Astrofis Arcetri, Florence, Italy.
[Umana, G.] INAF Osservatorio Astrofis Catania, Catania, Italy.
[Bonaldi, A.; de Zotti, G.; Massardi, M.] INAF Osservatorio Astron Padova, Padua, Italy.
[Polenta, G.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy.
[Burigana, C.; Butler, R. C.; Cuttaia, F.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Villa, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Paoletti, D.; Procopio, P.] INAF IASF Bologna, Bologna, Italy.
[Maino, D.; Bersanelli, M.; Tomasi, M.; Cappellini, B.; Donzelli, S.] INAF IASF Milano, Milan, Italy.
[Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France.
[Morisset, N.; Rohlfs, R.; Binko, P.; Meharga, M. T.; Tuerler, M.] Univ Geneva, ISDC Data Ctr Astrophys, Versoix, Switzerland.
[Chen, X.; Huynh, M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Puget, J. -L.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Bouchet, F. R.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France.
[Efstathiou, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Valiviita, J.; Donzelli, S.; Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Genova-Santos, R. T.; Gomez, F.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Lopez-Caniego, M.; Barreiro, R. B.; Curto, A.; Diego, J. M.; Herranz, D.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Gorski, K. M.; Keskitalo, R.; Lawrence, C. R.; Bartlett, J. G.; Colombo, L.; Gaier, T. C.; Jewell, J.; Mitra, S.; Pagano, L.; Pearson, D.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Leahy, J. P.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Watson, R.; Wilkinson, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
[Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Knoche, J.; Matthai, F.; Reinecke, M.; Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hell, R.; Hovest, W.; Rachen, J. P.; Robbers, G.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland.
[Baccigalupi, C.; Bonavera, L.; de Zotti, G.; Dick, J.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.; Danese, L.; Pettorino, V.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA.
[Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Zacchei, A (reprint author), INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, Trieste, Italy.
EM zacchei@oats.inaf.it
RI Butler, Reginald/N-4647-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014;
Gruppuso, Alessandro/N-5592-2015; Valiviita, Jussi/A-9058-2016;
Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Colombo,
Loris/J-2415-2016; bonavera, laura/E-9368-2017; Barreiro, Rita
Belen/N-5442-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Lilje,
Per/A-2699-2012; Salerno, Emanuele/A-2137-2010; de Gasperis,
Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego,
Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki,
Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti,
Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Cruz, Marcos/N-3429-2014
OI Watson, Robert/0000-0002-5873-0124; Zacchei, Andrea/0000-0003-0396-1192;
Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147;
Bouchet, Francois/0000-0002-8051-2924; Ricciardi,
Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta,
Samuele/0000-0002-3748-5115; TERENZI, LUCA/0000-0001-9915-6379; Umana,
Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis,
Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283;
Gregorio, Anna/0000-0003-4028-8785; Polenta,
Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996;
Sandri, Maura/0000-0003-4806-5375; Cuttaia,
Francesco/0000-0001-6608-5017; Burigana, Carlo/0000-0002-3005-5796;
Morgante, Gianluca/0000-0001-9234-7412; Maris,
Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591;
silk, joe/0000-0002-1566-8148; Matarrese, Sabino/0000-0002-2573-1243;
Pasian, Fabio/0000-0002-4869-3227; Finelli, Fabio/0000-0002-6694-3269;
Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso,
Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693;
Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi,
Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732;
bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose
Alberto/0000-0001-5289-3021; Vuerli, Claudio/0000-0002-9640-8785;
Melchiorri, Alessandro/0000-0001-5326-6003; Barreiro, Rita
Belen/0000-0002-6139-4272; Martinez-Gonzalez,
Enrique/0000-0002-0179-8590; Salerno, Emanuele/0000-0002-3433-3634; de
Gasperis, Giancarlo/0000-0003-2899-2171; Vielva,
Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386;
Herranz, Diego/0000-0003-4540-1417; Cruz, Marcos/0000-0002-4767-530X
FU European Space Agency (ESA) member states; CNES; CNRS/INSU-IN2P3; ASI;
INAF; Academy of Finland [121703, 121962]; EU within the DEISA Virtual
Community Support Initiative [RI-031513, RI-222919]; Spanish Ministerio
de Ciencia e Innovacion; Space Agency of the German Aerospace Center
(DLR) [50OP0901]; National Energy Research Scientific Computing Center;
Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]
FX Planck (http://www.esa.int/Planck) is a project of the European Space
Agency (ESA) with instruments provided by two scientific consortia
funded by ESA member states (in particular the lead countries France and
Italy), with contributions from NASA (USA) and telescope reflectors
provided by a collaboration between ESA and a scientific consortium led
and funded by Denmark.; Planck is too large a project to allow full
acknowledgement of all contributions by individuals, institutions,
industries, and funding agencies. The main entities involved in the
mission operations are as follows. The European Space Agency operates
the satellite via its Mission Operations Centre located at ESOC
(Darmstadt, Germany) and coordinates scientific operations via the
Planck Science Office located at ESAC (Madrid, Spain). Two Consortia,
comprising around 50 scientific institutes within Europe, the USA, and
Canada, and funded by agencies from the participating countries,
developed the scientific instruments LFI and HFI, and continue to
operate them via Instrument Operations Teams located in Trieste (Italy)
and Orsay (France). The Consortia are also responsible for scientific
processing of the acquired data. The Consortia are led by the Principal
Investigators: J.L. Puget in France for HFI (funded principally by CNES
and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI(funded
principally via ASI). NASA US Planck Project, based at J.P.L. and
involving scientists at many US institutions, contributes significantly
to the efforts of these two Consortia. The author list for this paper
has been selected by the Planck Science Team, and is composed of
individuals from all of the above entities who have made multi-year
contributions to the development of the mission. It does not pretend to
be inclusive of all contributions. The Planck-LFI project is developed
by an International Consortium lead by Italy and involving Canada,
Finland, Germany, Norway, Spain, Switzerland, UK, USA. The Italian
contribution to Planck is supported by the Italian Space Agency (ASI)
and INAF. This work was supported by the Academy of Finland grants
121703 and 121962. We thank the DEISA Consortium (http://www.deisa.eu),
co-funded through the EU FP6 project RI-031513 and the FP7 project
RI-222919, for support within the DEISA Virtual Community Support
Initiative. We thank CSC - IT Center for Science Ltd (Finland) for
computational resources. We acknowledge financial support provided by
the Spanish Ministerio de Ciencia e Innovacion through the Plan Nacional
del Espacio y Plan Nacional de Astronomia y Astrofisica. We acknowledge
The Max Planck Institute for Astrophysics Planck Analysis Centre (MPAC)
is funded by the Space Agency of the German Aerospace Center (DLR) under
grant 50OP0901 with resources of the German Federal Ministry of
Economics and Technology, and by the Max Planck Society. This work has
made use of the Planck satellite simulation package (Level-S), which is
assembled by the Max Planck Institute for Astrophysics Planck Analysis
Centre (MPAC) Reinecke et al. (2006). We acknowledge financial support
provided by the National Energy Research Scientific Computing Center,
which is supported by the Office of Science of the U.S. Department of
Energy under Contract No. DE-AC02-05CH11231. Some of the results in this
paper have been derived using the HEALPix package Gorski et al. (2005).
A description of the Planck Collaboration and a list of its members,
indicating which technical or scientific activities they have been
involved in, can be found at
http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborati
on.
NR 60
TC 74
Z9 74
U1 2
U2 9
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 DEC
PY 2011
VL 536
AR A5
DI 10.1051/0004-6361/201116484
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100006
ER
PT J
AU Peddle, DR
Huemmrich, KF
Hall, FG
Masek, JG
Soenen, SA
Jackson, CD
AF Peddle, Derek R.
Huemmrich, K. Fred
Hall, Forrest G.
Masek, Jeffrey G.
Soenen, Scott A.
Jackson, Chris D.
TI Applications of the BIOPHYS Algorithm for Physically-Based Retrieval of
Biophysical, Structural and Forest Disturbance Information
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Biophysical structure; BOREAS; canopy reflectance models; change; fire;
forest disturbance; harvest; inversion; Landsat; LEDAPS; MODIS
ID CANOPY REFLECTANCE MODEL; MULTIPLE-FORWARD-MODE; INVERSION;
CLASSIFICATION; SURFACE; VARIABLES
AB Canopy reflectance model inversion using look-up table approaches provides powerful and flexible options for deriving improved forest biophysical structural information (BSI) compared with traditional statistical empirical methods. The BIOPHYS algorithm is an improved, physically-based inversion approach for deriving BSI for independent use and validation and for monitoring, inventory and quantifying forest disturbance as well as input to ecosystem, climate and carbon models. Based on the multiple-forward mode (MFM) inversion approach, BIOPHYS results were summarised from different studies (Minnesota/NASA COVER; Virginia/LEDAPS; Saskatchewan/BOREAS), sensors (airborne MMR; Landsat; MODIS) and models (GeoSail; GOMS). Applications output included forest density, height, crown dimension, branch and green leaf area, canopy cover, disturbance estimates based on multi-temporal chronosequences, and structural change following recovery from forest fires over the last century. Good correspondences with validation field data were obtained. Integrated analyses of multiple solar and view angle imagery further improved retrievals compared with single pass data. Quantifying ecosystem dynamics such as the area and percent of forest disturbance, early regrowth and succession provide essential inputs to process-driven models of carbon flux. BIOPHYS is well suited for large-area, multi-temporal applications involving multiple image sets and mosaics for assessing vegetation disturbance and quantifying biophysical structural dynamics and change. It is also suitable for integration with forest inventory, monitoring, updating, and other programs.
C1 [Peddle, Derek R.; Soenen, Scott A.; Jackson, Chris D.] Univ Lethbridge, Dept Geog, Lethbridge, AB T1K 3M4, Canada.
[Peddle, Derek R.] Univ Lethbridge, ATIC, Lethbridge, AB T1K 3M4, Canada.
[Huemmrich, K. Fred; Hall, Forrest G.; Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Huemmrich, K. Fred; Hall, Forrest G.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol JCET, Baltimore, MD 21228 USA.
RP Peddle, DR (reprint author), Univ Lethbridge, Dept Geog, Water & Environm Sci Bldg, Lethbridge, AB T1K 3M4, Canada.
EM derek.peddle@uleth.ca
RI Masek, Jeffrey/D-7673-2012
FU NASA; Natural Sciences and Engineering Research Council of Canada
(NSERC); Alberta Ingenuity Centre for Water Research (AICWR);
NASA/LEDAPS; MODIS Science Team; Alberta Terrestrial Imaging Centre
(ATIC)
FX Manuscript received August 27, 2009; revised August 24, 2010; accepted
December 13, 2010. Date of publication September 15, 2011; date of
current version December 14, 2011. This work was supported by grants
from the NASA MODIS Science Program, the Natural Sciences and
Engineering Research Council of Canada (NSERC) and the Alberta Ingenuity
Centre for Water Research (AICWR), and also supported by NASA/LEDAPS,
the MODIS Science Team, and the Alberta Terrestrial Imaging Centre
(ATIC).
NR 37
TC 3
Z9 3
U1 2
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2011
VL 4
IS 4
BP 971
EP 982
DI 10.1109/JSTARS.2011.2164899
PG 12
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 861XR
UT WOS:000298054500029
ER
PT J
AU Shuler, RL
AF Shuler, Robert L., Jr.
TI Isotropy, equivalence, and the laws of inertia
SO PHYSICS ESSAYS
LA English
DT Article
DE Equivalence; Inertia; Mass; Acceleration; General Relativity; Gravity;
Precession; Light Bending; Mach; Isotropy
ID ANISOTROPY; SEARCH
AB An analysis of the appearance of time and motion in an accelerated frame gives the result expected by Einstein and others of an apparent mass increase in proportion to potential. This leads to a set of transformations we call the laws of inertia. The resulting inertia is isotropic. One can infer that these results apply to a gravitational field due to the Einstein equivalence principle. This removes an objection to Mach's principle based on possible anisotropy. Further exploring the gravitational analogy reveals nonphysical properties the analogy must have for an acceleration to be "equivalent" to gravity for weak field effects such as precession and light bending. The new formulation, modified equivalence, clarifies the literature about what is or is not derivable from equivalence by showing exactly where the deficiency lies in ordinary equivalence, without resorting to Riemannian mathematics. (C) 2011 Physics Essays Publication. [DOI: 10.4006/1.3637365]
C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Shuler, RL (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM robert.l.shuler@nasa.gov
NR 29
TC 0
Z9 0
U1 1
U2 3
PU PHYSICS ESSAYS PUBLICATION
PI OTTAWA
PA PO BOX 8141 STATION T, OTTAWA, ONTARIO K1G 3H6, CANADA
SN 0836-1398
J9 PHYS ESSAYS
JI Phys. Essays
PD DEC
PY 2011
VL 24
IS 4
BP 498
EP 507
DI 10.4006/1.3637365
PG 10
WC Physics, Multidisciplinary
SC Physics
GA 879ZB
UT WOS:000299372200007
ER
PT J
AU Zenitani, S
Hesse, M
Klimas, A
Black, C
Kuznetsova, M
AF Zenitani, Seiji
Hesse, Michael
Klimas, Alex
Black, Carrie
Kuznetsova, Masha
TI The inner structure of collisionless magnetic reconnection: The
electron-frame dissipation measure and Hall fields
SO PHYSICS OF PLASMAS
LA English
DT Article
ID DIFFUSION REGION; MAGNETOTAIL; INSTABILITY; CHALLENGE; PLASMA; SYSTEM
AB It was recently proposed that the electron-frame dissipation measure, the energy transfer from the electromagnetic field to plasmas in the electron's rest frame, identifies the dissipation region of collisionless magnetic reconnection [Zenitani , Phys. Rev. Lett. 106, 195003 (2011)]. The measure is further applied to the electron-scale structures of antiparallel reconnection, by using two-dimensional particle-in-cell simulations. The size of the central dissipation region is controlled by the electron-ion mass ratio, suggesting that electron physics is essential. A narrow electron jet extends along the outflow direction until it reaches an electron shock. The jet region appears to be anti-dissipative. At the shock, electron heating is relevant to a magnetic cavity signature. The results are summarized to a unified picture of the single dissipation region in a Hall magnetic geometry. (C) 2011 American Institute of Physics. [doi:10.1063/1.3662430]
C1 [Zenitani, Seiji; Hesse, Michael; Klimas, Alex; Black, Carrie; Kuznetsova, Masha] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zenitani, S (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
EM seiji.zenitani@nao.ac.jp
RI Hesse, Michael/D-2031-2012; Kuznetsova, Maria/F-6840-2012; 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 JSPS; NASA
FX The authors acknowledge Keizo Fujimoto and Nicolas Aunai for useful
comments. One of the authors (S.Z.) acknowledges support from JSPS
Postdoctoral Fellowships for Research Abroad. This work was supported by
NASA's MMS mission.
NR 33
TC 18
Z9 18
U1 0
U2 8
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD DEC
PY 2011
VL 18
IS 12
AR 122108
DI 10.1063/1.3662430
PG 9
WC Physics, Fluids & Plasmas
SC Physics
GA 870AX
UT WOS:000298642600010
ER
PT J
AU Tchebakova, NM
Parfenova, EI
Soja, AJ
AF Tchebakova, N. M.
Parfenova, E. I.
Soja, A. J.
TI Climate change and climate-induced hot spots in forest shifts in central
Siberia from observed data
SO REGIONAL ENVIRONMENTAL CHANGE
LA English
DT Article
DE Instrumental climate record; IPCC climate change projections; Forest
shift; Siberia
ID NORTHERN EURASIA; WHITE SPRUCE; FIRE; 20TH-CENTURY; GROWTH; ALASKA;
COVER; SNOW
AB Regional Siberian studies have already registered climate warming over the last several decades. We evaluated ongoing climate change in central Siberia between 1991 and 2010 and a baseline period, 1961-1990, and between 1991 and 2010 and Hadley 2020 climate change projections, represented by the moderate B1 and severe A2 scenarios. Our analysis showed that winters are already 2-3A degrees C warmer in the north and 1-2A degrees C warmer in the south by 2010. Summer temperatures increased by 1A degrees C in the north and by 1-2A degrees C in the south. Change in precipitation is more complicated, increasing on average 10% in middle latitudes and decreasing 10-20% in the south, promoting local drying in already dry landscapes. Hot spots of possible forest shifts are modeled using our Siberian bioclimatic vegetation model and mountain vegetation model with respect to climate anomalies observed pre-2010 and predicted 2020 Hadley scenarios. Forests are predicted to shift northwards along the central Siberian Plateau and upslope in both the northern and southern mountains. South of the central Siberian Plateau, steppe advancement is predicted that was previously non-existent north of 56A degrees N latitude. South of 56A degrees N, steppe expansion is predicted in the dry environments of Khakasiya and Tyva. In the southern mountains, it is predicted that the lower tree line will migrate upslope due to increased dryness in the intermontane Tyvan basins. The hot spots of vegetation change that are predicted by our models are confirmed by regional literature data.
C1 [Tchebakova, N. M.; Parfenova, E. I.] Russian Acad Sci Academgorodok, VN Sukachev Inst Forest, Siberian Branch, Krasnoyarsk 660036, Russia.
[Soja, A. J.] NASA Langley Res Ctr, Natl Inst Aerosp, Hampton, VA 23681 USA.
RP Tchebakova, NM (reprint author), Russian Acad Sci Academgorodok, VN Sukachev Inst Forest, Siberian Branch, Krasnoyarsk 660036, Russia.
EM ncheby@ksc.krasn.ru
FU Russian Foundation for Basic Research [10-05-00941]; NASA
[09-IDS09-0116]
FX This study was supported by grant #10-05-00941 of the Russian Foundation
for Basic Research and NASA Research Opportunities in Space and Earth
Sciences (ROSES) 2009 InterDisciplinary Science (IDS) 09-IDS09-0116.
NR 65
TC 17
Z9 18
U1 2
U2 16
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1436-3798
J9 REG ENVIRON CHANGE
JI Reg. Envir. Chang.
PD DEC
PY 2011
VL 11
IS 4
BP 817
EP 827
DI 10.1007/s10113-011-0210-4
PG 11
WC Environmental Sciences; Environmental Studies
SC Environmental Sciences & Ecology
GA 864GT
UT WOS:000298226500007
ER
PT J
AU Gershman, DJ
Block, BP
Rubin, M
Benna, M
Mahaffy, PR
Zurbuchen, TH
AF Gershman, D. J.
Block, B. P.
Rubin, M.
Benna, M.
Mahaffy, P. R.
Zurbuchen, T. H.
TI Higher order parametric excitation modes for spaceborne quadrupole mass
spectrometers
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
DE aircraft instrumentation; field programmable gate arrays; mass
spectrometer accessories; mass spectrometers; robust control; voltage
control
ID ION-TRAP; FILTER; ATMOSPHERE; STABILITY; FIELD
AB This paper describes a technique to significantly improve upon the mass peak shape and mass resolution of spaceborne quadrupole mass spectrometers (QMSs) through higher order auxiliary excitation of the quadrupole field. Using a novel multiresonant tank circuit, additional frequency components can be used to drive modulating voltages on the quadrupole rods in a practical manner, suitable for both improved commercial applications and spaceflight instruments. Auxiliary excitation at frequencies near twice that of the fundamental quadrupole RF frequency provides the advantages of previously studied parametric excitation techniques, but with the added benefit of increased sensed excitation amplitude dynamic range and the ability to operate voltage scan lines through the center of upper stability islands. Using a field programmable gate array, the amplitudes and frequencies of all QMS signals are digitally generated and managed, providing a robust and stable voltage control system. These techniques are experimentally verified through an interface with a commercial Pfeiffer QMG422 quadrupole rod system. When operating through the center of a stability island formed from higher order auxiliary excitation, approximately 50% and 400% improvements in 1% mass resolution and peak stability were measured, respectively, when compared with traditional QMS operation. Although tested with a circular rod system, the presented techniques have the potential to improve the performance of both circular and hyperbolic rod geometry QMS sensors. (C) 2011 American Institute of Physics. [doi:10.1063/1.3669781]
C1 [Gershman, D. J.; Block, B. P.; Rubin, M.; Zurbuchen, T. H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Benna, M.; Mahaffy, P. R.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gershman, DJ (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RI Benna, Mehdi/F-3489-2012; Rubin, Martin/I-7777-2013
OI Rubin, Martin/0000-0001-6549-3318
FU NASA [PIDDP NNX08AO05G, GSRP NNX09AL50H]
FX The authors would like to acknowledge the support of the NASA PIDDP
NNX08AO05G and NASA GSRP NNX09AL50H grants that made this work possible.
The University of Michigan is pursuing patent protection for the
presented intellectual property and is seeking commercialization
partners to help bring the technology to market.
NR 29
TC 3
Z9 3
U1 1
U2 15
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD DEC
PY 2011
VL 82
IS 12
AR 125109
DI 10.1063/1.3669781
PG 15
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 870BC
UT WOS:000298643100062
PM 22225251
ER
PT J
AU Sanjuan, J
Preston, A
Korytov, D
Spector, A
Freise, A
Dixon, G
Livas, J
Mueller, G
AF Sanjuan, J.
Preston, A.
Korytov, D.
Spector, A.
Freise, A.
Dixon, G.
Livas, J.
Mueller, G.
TI Carbon fiber reinforced polymer dimensional stability investigations for
use on the laser interferometer space antenna mission telescope
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
DE astronomical telescopes; gravitational wave detectors; gravitational
waves; mirrors
ID FREQUENCY STABILIZATION; MOLECULAR-IODINE; YAG LASER; ND
AB The laser interferometer space antenna (LISA) is a mission designed to detect low frequency gravitational waves. In order for LISA to succeed in its goal of direct measurement of gravitational waves, many subsystems must work together to measure the distance between proof masses on adjacent spacecraft. One such subsystem, the telescope, plays a critical role as it is the laser transmission and reception link between spacecraft. Not only must the material that makes up the telescope support structure be strong, stiff, and light, but it must have a dimensional stability of better than 1 pm Hz (1/2) at 3 mHz and the distance between the primary and the secondary mirrors must change by less than 2.5 mu m over the mission lifetime. Carbon fiber reinforced polymer is the current baseline material; however, it has not been tested to the pico meter level as required by the LISA mission. In this paper, we present dimensional stability results, outgassing effects occurring in the cavity and discuss its feasibility for use as the telescope spacer for the LISA spacecraft. (C) 2011 American Institute of Physics. [doi: 10.1063/1.3662470]
C1 [Sanjuan, J.; Korytov, D.; Spector, A.; Mueller, G.] Univ Florida, Gainesville, FL 32611 USA.
[Preston, A.; Livas, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Freise, A.; Dixon, G.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
RP Sanjuan, J (reprint author), Univ Florida, Corner Gale Lemerand Dr & Museum Rd, Gainesville, FL 32611 USA.
RI Livas, Jeffrey/D-2994-2012; Dixon, George/K-5501-2014;
OI Freise, Andreas/0000-0001-6586-9901
NR 25
TC 5
Z9 6
U1 0
U2 7
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD DEC
PY 2011
VL 82
IS 12
AR 124501
DI 10.1063/1.3662470
PG 11
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 870BC
UT WOS:000298643100045
PM 22225234
ER
PT J
AU Bisi, MM
Thompson, BJ
Emery, BA
Gibson, SE
Leibacher, J
van Driel-Gesztelyi, L
AF Bisi, Mario M.
Thompson, Barbara J.
Emery, Barbara A.
Gibson, Sarah E.
Leibacher, John
van Driel-Gesztelyi, Lidia
TI The Sun-Earth Connection near Solar Minimum: Placing it into Context
SO SOLAR PHYSICS
LA English
DT Editorial Material
C1 [Bisi, Mario M.] Aberystwyth Univ, Aberystwyth, Dyfed, Wales.
[Thompson, Barbara J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Emery, Barbara A.; Gibson, Sarah E.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA.
[Leibacher, John] Natl Solar Observ, Tucson, AZ 85719 USA.
[Leibacher, John] Inst Astrophys Spatiale, Orsay, France.
[van Driel-Gesztelyi, Lidia] Univ Paris 06, LESIA Observat Paris, CNRS, Univ Paris Diderot, Meudon, France.
[van Driel-Gesztelyi, Lidia] Univ Coll London, Mullard Space Sci Lab, Holmbury RH5 6NT, England.
[van Driel-Gesztelyi, Lidia] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary.
RP Bisi, MM (reprint author), Aberystwyth Univ, Aberystwyth, Dyfed, Wales.
EM Mario.Bisi@aber.ac.uk; barbara.j.thompson@nasa.gov; emery@ucar.edu;
sgibson@ucar.edu; john.leibacher@gmail.com; Lidia.vanDriel@obspm.fr
RI Thompson, Barbara/C-9429-2012;
OI Leibacher, John/0000-0001-7605-3684
NR 0
TC 3
Z9 3
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD DEC
PY 2011
VL 274
IS 1-2
BP 1
EP 3
DI 10.1007/s11207-011-9915-2
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873ER
UT WOS:000298864400001
ER
PT J
AU Gibson, SE
de Toma, G
Emery, B
Riley, P
Zhao, L
Elsworth, Y
Leamon, RJ
Lei, J
McIntosh, S
Mewaldt, RA
Thompson, BJ
Webb, D
AF Gibson, S. E.
de Toma, G.
Emery, B.
Riley, P.
Zhao, L.
Elsworth, Y.
Leamon, R. J.
Lei, J.
McIntosh, S.
Mewaldt, R. A.
Thompson, B. J.
Webb, D.
TI The Whole Heliosphere Interval in the Context of a Long and Structured
Solar Minimum: An Overview from Sun to Earth
SO SOLAR PHYSICS
LA English
DT Article
ID DOUBLE MAGNETIC CYCLE; CORONAL HOLES; FIELD; MASS
AB Throughout months of extremely low solar activity during the recent extended solar-cycle minimum, structural evolution continued to be observed from the Sun through the solar wind and to the Earth. In 2008, the presence of long-lived and large low-latitude coronal holes meant that geospace was periodically impacted by high-speed streams, even though solar irradiance, activity, and interplanetary magnetic fields had reached levels as low as, or lower than, observed in past minima. This time period, which includes the first Whole Heliosphere Interval (WHI 1: Carrington Rotation (CR) 2068), illustrates the effects of fast solar-wind streams on the Earth in an otherwise quiet heliosphere. By the end of 2008, sunspots and solar irradiance had reached their lowest levels for this minimum (e.g., WHI 2: CR 2078), and continued solar magnetic-flux evolution had led to a flattening of the heliospheric current sheet and the decay of the low-latitude coronal holes and associated Earth-intersecting high-speed solar-wind streams. As the new solar cycle slowly began, solar-wind and geospace observables stayed low or continued to decline, reaching very low levels by June -aEuro parts per thousand July 2009. At this point (e.g., WHI 3: CR 2085) the Sun-Earth system, taken as a whole, was at its quietest. In this article we present an overview of observations that span the period 2008 -aEuro parts per thousand 2009, with highlighted discussion of CRs 2068, 2078, and 2085. We show side-by-side observables from the Sun's interior through its surface and atmosphere, through the solar wind and heliosphere and to the Earth's space environment and upper atmosphere, and reference detailed studies of these various regimes within this topical issue and elsewhere.
C1 [Gibson, S. E.; de Toma, G.; Emery, B.; Zhao, L.; McIntosh, S.] NCAR HAO, Boulder, CO USA.
[Riley, P.] Predict Sci Inc, San Diego, CA USA.
[Elsworth, Y.] Univ Birmingham, Birmingham, W Midlands, England.
[Leamon, R. J.] Montana State Univ, Bozeman, MT 59717 USA.
[Lei, J.] Univ Sci & Technol China, Beijing, Peoples R China.
[Mewaldt, R. A.] CALTECH, Pasadena, CA 91125 USA.
[Thompson, B. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Webb, D.] Boston Coll, Boston, MA USA.
RP Gibson, SE (reprint author), NCAR HAO, Boulder, CO USA.
EM sgibson@ucar.edu; detoma@ucar.edu; emery@ucar.edu; pete@predsci.com;
lzh@ucar.edu; ype@bison.ph.bham.ac.uk; robert.j.leamon@nasa.gov;
leijh@ustc.edu.cn; mscott@ucar.edu; mewaldt@srl.caltech.edu;
barbara.j.thompson@nasa.gov; david.webb@bc.edu
RI Zhao, Liang/B-8215-2012; Thompson, Barbara/C-9429-2012; Lei,
Jiuhou/A-3015-2012;
OI Lei, Jiuhou/0000-0002-4374-5083; Zhao, Liang/0000-0002-5975-7476
FU National Science Foundation; Chinese Academy of Science; NASA
FX We thank Todd Hoeksema, Marc DeRosa, Alysha Reinard, and Larisza Krista
for useful discussions. The hourly solar-wind plasma and IMF data were
taken from the OMNI-2 collection from the Space Physics Data Facility at
the Goddard Space Flight Center managed by Natalia Papitashvili. This
study used indices from the CEDAR Database at the National Center for
Atmospheric Research (NCAR), which is supported by the National Science
Foundation. J. Lei thanks Eric Sutton for providing CHAMP data and
support from the 100 Talents Program of the Chinese Academy of Science.
SOHO is a project of international collaboration between ESA and NASA.
We gratefully acknowledge the use of the SolarSoft package for
generating PFSS fields developed by Marc DeRosa. Radiation-belt
electron-number fluxes from the GOES satellites come from NGDC via SPIDR
at http://spidr.ngdc.noaa.gov starting with GOES-05 in January 1986 and
extending through GOES-12. We thank Terry Onsager for his comments and
assistance with these data. We also thank Anne-Marie Broomhall for
assistance with the BiSON data, and Thomas Kuchar for assistance with
the CACTus CME data. The research of L. Zhao is supported by the NASA
Living with a Star Heliophysics Postdoctoral Fellowship Program,
administered by the University Corporation for Atmospheric Research.
NR 60
TC 28
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U1 1
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD DEC
PY 2011
VL 274
IS 1-2
BP 5
EP 27
DI 10.1007/s11207-011-9921-4
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873ER
UT WOS:000298864400002
ER
PT J
AU Thompson, BJ
Gibson, SE
Schroeder, PC
Webb, DF
Arge, CN
Bisi, MM
de Toma, G
Emery, BA
Galvin, AB
Haber, DA
Jackson, BV
Jensen, EA
Leamon, RJ
Lei, JH
Manoharan, PK
Mays, ML
McIntosh, PS
Petrie, GJD
Plunkett, SP
Qian, LY
Riley, P
Suess, ST
Tokumaru, M
Welsch, BT
Woods, TN
AF Thompson, Barbara J.
Gibson, Sarah E.
Schroeder, Peter C.
Webb, David F.
Arge, Charles N.
Bisi, Mario M.
de Toma, Giuliana
Emery, Barbara A.
Galvin, Antoinette B.
Haber, Deborah A.
Jackson, Bernard V.
Jensen, Elizabeth A.
Leamon, Robert J.
Lei, Jiuhou
Manoharan, Periasamy K.
Mays, M. Leila
McIntosh, Patrick S.
Petrie, Gordon J. D.
Plunkett, Simon P.
Qian, Liying
Riley, Peter
Suess, Steven T.
Tokumaru, Munetoshi
Welsch, Brian T.
Woods, Thomas N.
TI A Snapshot of the Sun Near Solar Minimum: The Whole Heliosphere Interval
SO SOLAR PHYSICS
LA English
DT Article
ID MAGNETIC-FIELD; WIND; PREDICTION; DYNAMICS
AB We present an overview of the data and models collected for the Whole Heliosphere Interval, an international campaign to study the three-dimensional solar-heliospheric-planetary connected system near solar minimum. The data and models correspond to solar Carrington Rotation 2068 (20 March -aEuro parts per thousand 16 April 2008) extending from below the solar photosphere, through interplanetary space, and down to Earth's mesosphere. Nearly 200 people participated in aspects of WHI studies, analyzing and interpreting data from nearly 100 instruments and models in order to elucidate the physics of fundamental heliophysical processes. The solar and inner heliospheric data showed structure consistent with the declining phase of the solar cycle. A closely spaced cluster of low-latitude active regions was responsible for an increased level of magnetic activity, while a highly warped current sheet dominated heliospheric structure. The geospace data revealed an unusually high level of activity, driven primarily by the periodic impingement of high-speed streams. The WHI studies traced the solar activity and structure into the heliosphere and geospace, and provided new insight into the nature of the interconnected heliophysical system near solar minimum.
C1 [Gibson, Sarah E.; de Toma, Giuliana; Emery, Barbara A.; Qian, Liying] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Mays, M. Leila] NASA, Goddard Space Flight Ctr, ORAU, Greenbelt, MD 20771 USA.
[Schroeder, Peter C.; Welsch, Brian T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Webb, David F.] Boston Coll, ISR, Newton, MA USA.
[Arge, Charles N.] Hanscom AFB Res Lab, Hanscom AFB, MA USA.
[Bisi, Mario M.; Jackson, Bernard V.; Jensen, Elizabeth A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Bisi, Mario M.] Aberystwyth Univ, Inst Math & Phys, Aberystwyth, Dyfed, Wales.
[Galvin, Antoinette B.] Univ New Hampshire, EOS, Durham, NH 03824 USA.
[Haber, Deborah A.] Univ Colorado, JILA, Boulder, CO 80309 USA.
[Leamon, Robert J.] Montana State Univ, Bozeman, MT 59717 USA.
[Lei, Jiuhou] Univ Sci & Technol China, Sch Earth & Space Sci, Hefei 230026, Peoples R China.
[Manoharan, Periasamy K.] Tata Inst Fundamental Res, Radio Astron Ctr, Ooty, Tamil Nadu, India.
[McIntosh, Patrick S.] Heliosynoptics Inc, Boulder, CO USA.
[Petrie, Gordon J. D.] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA.
[Plunkett, Simon P.] USN, Res Lab, Washington, DC 20375 USA.
[Riley, Peter] Predict Sci, San Diego, CA USA.
[Suess, Steven T.] Natl Space Sci & Technol Ctr, Huntsville, AL USA.
[Tokumaru, Munetoshi] Nagoya Univ, STELab, Nagoya, Aichi 4648601, Japan.
[Woods, Thomas N.] Univ Colorado, LASP, Boulder, CO 80309 USA.
RP Gibson, SE (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA.
EM sgibson@ucar.edu
RI Thompson, Barbara/C-9429-2012; Lei, Jiuhou/A-3015-2012; Galvin,
Antoinette/A-6114-2013; Qian, Liying/D-9236-2013;
OI Manoharan, Periasamy K/0000-0003-4274-211X; Lei,
Jiuhou/0000-0002-4374-5083; Qian, Liying/0000-0003-2430-1388; Petrie,
Gordon/0000-0001-8462-9161
FU National Science Foundation [ATM-0608577]; NASA [NASA NNH08ZDA001N-HGI]
FX The authors extend their sincere gratitude to the following for useful
discussions and/or assistance in providing data/models/results used in
this publication: A. Balogh, Ulysses/VHM Principal Investigator,
Imperial College of Science, Technology and Medicine, London (UK); J.M.
Clover and P.P. Hick, University of California, San Diego (USA); J.
Davies, Rutherford Appleton Laboratory (UK); Andrew Davis, ACE Science
Center at Caltech (USA); R.A. Fallows, Aberystwyth University, Wales
(UK); R. Fuller-Rowell, T. Onsager, and A. Reinard, NOAA/SWPC, Boulder
(USA); Nat Gopalswamy, NASA/GSFC, GreenbeltMD(USA); J. T. Gosling,
University of Colorado, Boulder (USA); J.U. Kozyra, University of
Michigan, Ann Arbor (USA); M. Lancaster and C. Tranquille, Ulysses Data
System, ESA/ESTEC (Netherlands); J.G. Luhmann, STEREO/IMPACT Principal
Investigator, UC Berkeley/SSL (USA); D. J. McComas, Ulysses/SWOOPS
Principal Investigator, Southwest Research Institute (USA); S.W.
McIntosh and S. Solomon, UCAR/HAO, Boulder (USA); M. Mlynczak,
NASA/Langley Research Center and the TIMED/SABER team; J. Sojka, Utah
State University (USA); A. Szabo, Wind Project Scientist, NASA/GSFC
(USA). The electron auroral power data were supplied by the Coupling,
Energetics and Dynamics of Atmospheric Regions (CEDAR) Database, which
is supported by the National Science Foundation.; The National Center
for Atmospheric Research is supported through the National Science
Foundation. FISR is operated by SRI International under NSF cooperative
agreement ATM-0608577. L. Qian's effort was supported by NASA
Heliophysics Guest Investigator Grant #NASA NNH08ZDA001N-HGI.
NR 62
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U1 0
U2 3
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 DEC
PY 2011
VL 274
IS 1-2
BP 29
EP 56
DI 10.1007/s11207-011-9891-6
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873ER
UT WOS:000298864400003
ER
PT J
AU Webb, DF
Cremades, H
Sterling, AC
Mandrini, CH
Dasso, S
Gibson, SE
Haber, DA
Komm, RW
Petrie, GJD
McIntosh, PS
Welsch, BT
Plunkett, SP
AF Webb, D. F.
Cremades, H.
Sterling, A. C.
Mandrini, C. H.
Dasso, S.
Gibson, S. E.
Haber, D. A.
Komm, R. W.
Petrie, G. J. D.
McIntosh, P. S.
Welsch, B. T.
Plunkett, S. P.
TI The Global Context of Solar Activity During the Whole Heliosphere
Interval Campaign
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal mass ejections, origins; Solar synoptic maps; Helioseismology,
subsurface flows
ID CORONAL MASS EJECTION; MAGNETIC-FIELDS; SUBSURFACE FLOWS; CURRENT
MINIMUM; REGIONS; FLARES; RECONSTRUCTION; VORTICITY; DYNAMICS; HOLES
AB The Whole Heliosphere Interval (WHI) was an international observing and modeling effort to characterize the 3-D interconnected "heliophysical" system during this solar minimum, centered on Carrington Rotation 2068, March 20 -aEuro parts per thousand April 16, 2008. During the latter half of the WHI period, the Sun presented a sunspot-free, deep solar minimum type face. But during the first half of CR 2068 three solar active regions flanked by two opposite-polarity, low-latitude coronal holes were present. These departures from the quiet Sun led to both eruptive activity and solar wind structure. Most of the eruptive activity, i.e., flares, filament eruptions and coronal mass ejections (CMEs), occurred during this first, active half of the interval. We determined the source locations of the CMEs and the type of associated region, such as active region, or quiet sun or active region prominence. To analyze the evolution of the events in the context of the global solar magnetic field and its evolution during the three rotations centered on CR 2068, we plotted the CME source locations onto synoptic maps of the photospheric magnetic field, of the magnetic and chromospheric structure, of the white light corona, and of helioseismological subsurface flows. Most of the CME sources were associated with the three dominant active regions on CR 2068, particularly AR 10989. Most of the other sources on all three CRs appear to have been associated with either isolated filaments or filaments in the north polar crown filament channel. Although calculations of the flux balance and helicity of the surface magnetic features did not clearly identify a dominance of one region over the others, helioseismological subsurface flows beneath these active regions did reveal a pronounced difference among them. These preliminary results suggest that the "twistedness" (i.e., vorticity and helicity) of subsurface flows and its temporal variation might be related to the CME productivity of active regions, similar to the relationship between flares and subsurface flows.
C1 [Webb, D. F.] Boston Coll, ISR, Chestnut Hill, MA 02167 USA.
[Cremades, H.] UTN FRM CONICET, Mendoza, Argentina.
[Sterling, A. C.] NASA MSFC, Huntsville, AL USA.
[Mandrini, C. H.; Dasso, S.] Consejo Nacl Invest Cient & Tecn, IAFE, RA-1033 Buenos Aires, DF, Argentina.
[Mandrini, C. H.] Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Fis, RA-1428 Buenos Aires, DF, Argentina.
[Gibson, S. E.] NCAR High Altitude Observ, Boulder, CO USA.
[Haber, D. A.] Univ Colorado, JILA, Boulder, CO 80309 USA.
[Komm, R. W.; Petrie, G. J. D.] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA.
[McIntosh, P. S.] Heliosynoptics Inc, Boulder, CO USA.
[Welsch, B. T.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA.
[Plunkett, S. P.] USN, Res Lab, Washington, DC 20375 USA.
RP Webb, DF (reprint author), Boston Coll, ISR, Chestnut Hill, MA 02167 USA.
EM david.webb@bc.edu
FU ANPCyT [PICT2007-1790, PICT 2007-00856]; NASA [NNH08AH251]; CONICET
[PIP-2009-00825]; NSF SHINE [ATM-0752597]; NCAR; AF [FA8718-06-C-0015,
FA8718-10-C-0001]; Navy [N00173-07-1-G016, N00173-10-1-G001]
FX Additional Contributors to the Global WHI CME Studies were J. Davies, B.
Jackson, A. Kosovichev, P. Lisnichenko, and O. Podladchikova. H. C.,
S.D., and C.H.M. are members of the Carrera del Investigador Cient fico,
CONICET. H.C. and C.H.M. acknowledge financial support from ANPCyT
through grant PICT2007-1790. A.C.S received funding from NASA's Science
Mission Directorate through the Solar Physics Supporting Research and
Technology Program. G.P. acknowledges funding from NASA Grant
NNH08AH251. S.D. thanks the Argentinean grants PICT 2007-00856 (ANPCyT)
and PIP-2009-00825 (CONICET). B. T.W. acknowledges support of NSF SHINE
award ATM-0752597. S.E. G. thanks the NSF, which sponsors NCAR. D.F.W
was supported by AF contracts FA8718-06-C-0015 and FA8718-10-C-0001 and
Navy contracts N00173-07-1-G016 and N00173-10-1-G001. The GONG program
is managed by NSO. NSO is operated by AURA, Inc. under a cooperative
agreement with the NSF. The GONG data were acquired by instruments
operated by the Big Bear Solar Observatory, High Altitude Observatory,
Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de
Astrofisica de Canarias, and Cerro Tololo Interamerican Observatory.
SOLIS/VSM vector magnetograms are produced cooperatively by NSF/NSO and
NASA/LWS. EIT, LASCO, and MDI data are courtesy of the SOHO/EIT,
SOHO/LASCO, and SOHO/MDI consortia. SOHO is a project of international
cooperation between ESA and NASA. SECCHI data are courtesy of the
STEREO/SECCHI consortium.
NR 52
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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 DEC
PY 2011
VL 274
IS 1-2
BP 57
EP 86
DI 10.1007/s11207-011-9787-5
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873ER
UT WOS:000298864400004
ER
PT J
AU Welsch, BT
Christe, S
McTiernan, JM
AF Welsch, B. T.
Christe, S.
McTiernan, J. M.
TI Photospheric Magnetic Evolution in the WHI Active Regions
SO SOLAR PHYSICS
LA English
DT Article
DE Flares, dynamics; Helicity, magnetic; Magnetic fields, corona
ID CORONAL MASS EJECTIONS; LOCAL CORRELATION TRACKING; MAJOR SOLAR-FLARES;
INDUCTION EQUATION; HELICITY INJECTION; FLUX CANCELLATION; QUIET SUN;
FIELD; MAGNETOGRAMS; ENERGY
AB Sequences of line-of-sight (LOS) magnetograms recorded by the Michelson Doppler Imager are used to quantitatively characterize photospheric magnetic structure and evolution in three active regions that rotated across the Sun's disk during the Whole Heliosphere Interval (WHI), in an attempt to relate the photospheric magnetic properties of these active regions to flares and coronal mass ejections (CMEs). Several approaches are used in our analysis, on scales ranging from whole active regions, to magnetic features, to supergranular scales, and, finally, to individual pixels. We calculated several parameterizations of magnetic structure and evolution that have previously been associated with flare and CME activity, including total unsigned magnetic flux, magnetic flux near polarity-inversion lines, amount of canceled flux, the "proxy Poynting flux," and helicity flux. To catalog flare events, we used flare lists derived from both GOES and RHESSI observations. By most such measures, AR 10988 should have been the most flare- and CME-productive active region, and AR 10989 the least. Observations, however, were not consistent with this expectation: ARs 10988 and 10989 produced similar numbers of flares, and AR 10989 also produced a few CMEs. These results highlight present limitations of statistics-based flare and CME forecasting tools that rely upon line-of-sight photospheric magnetic data alone.
C1 [Welsch, B. T.; McTiernan, J. M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christe, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Welsch, BT (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM welsch@ssl.berkeley.edu
OI Christe, Steven/0000-0001-6127-795X
FU American taxpayers; NASA [NAS5-98033, NNX08AJ18G, NNX08AI56G]; NSF
[ATM-0752597, AGS-1024862]
FX The authors owe thanks to many people: the WHI Team for inviting BTW to
participate in the Second WHI Workshop; the organizers of this Topical
Issue of Solar Physics; the SOHO/MDI and RHESSI teams for making their
databases available and easy to use; and the American taxpayers, for
their financial support of this work. MDI is funded through NASA's Solar
and Heliospheric Physics program; SOHO is a project of international
cooperation between ESA and NASA. This research has made use of NASA's
Astrophysics Data System Service. BTW acknowledges support from NSF
awards ATM-0752597 and AGS-1024862. JMM acknowledges support from NASA
grants NAS5-98033, NNX08AJ18G and NNX08AI56G.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
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EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD DEC
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VL 274
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
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UT WOS:000298864400008
ER
PT J
AU Echer, E
Tsurutani, BT
Gonzalez, WD
Kozyra, JU
AF Echer, E.
Tsurutani, B. T.
Gonzalez, W. D.
Kozyra, J. U.
TI High Speed Stream Properties and Related Geomagnetic Activity During the
Whole Heliosphere Interval (WHI): 20 March to 16 April 2008
SO SOLAR PHYSICS
LA English
DT Article
DE Solar wind; High-speed streams; Geomagnetic activity; Solar cycle; Space
weather; Whole heliosphere interval; Alfven waves; Nested variances
ID SOLAR-WIND STREAMS; INTERPLANETARY MAGNETIC FIELD; CORONAL MASS
EJECTIONS; ALFVEN WAVES; INTERACTION REGIONS; COROTATING SHOCKS;
DECLINING PHASE; STORMS; CYCLE; MAGNETOSPHERE
AB We study the interplanetary features and concomitant geomagnetic activity of the two high-speed streams (HSSs) selected by the Whole Heliosphere Interval (WHI) campaign participants: 20 March to 16 April 2008 in Carrington rotation (CR) 2068. This interval was chosen to perform a comprehensive study of HSSs and their geoeffectiveness during this "deep" solar minimum. The two HSSs within the interval were characterized by fast solar-wind speeds (peak values > 600 km s(-1)) containing large-amplitude Alfv,nic fluctuations, as is typical of HSSs during normal solar minima. However, the interplanetary magnetic field (IMF) magnitude [B (o)] was exceptionally low (a parts per thousand 3 -aEuro parts per thousand 5 nT) during these HSSs, leading to lower than usual IMF B (z) values. The first HSS (HSS1) had favorable IMF polarity for geomagnetic activity (negative during northern Spring). The average AE and Dst for the HSS1 proper (HSS1P) were + 258 nT and -aEuro parts per thousand 21 nT, respectively. The second HSS (HSS2) had a positive sector IMF polarity, one that is less favorable for geomagnetic activity. The AE and Dst index averages were + 188 nT and -aEuro parts per thousand 7 nT, both lower than corresponding numbers for the first event, as expected. The HSS1P geomagnetic activity is comparable to, and the HSS2P geomagnetic activity lower than, corresponding observations for the previous minimum (1996). Both events' geomagnetic activities are lower than HSS events previously studied in the declining phase (in 2003). In general, V (sw) was faster for the HSSs in 2008 compared to 1996. The southward IMF B (z) was lower in the former. The product of these two parameters [V (sw) and IMF B (z) ] comprises the solar-wind electric field, which is most directly associated with the energy input into the magnetosphere during the HSS intervals. Thus the combined effects led to the solar wind energy input in 2008 being slightly less than that in 1996. A detailed analysis of magnetic-field variances and Alfv,nicity is performed to explore the characteristics of Alfv,n waves (a central element in the geoeffectiveness of HSSs) during the WHI. The B (z) variances in the proto-CIR (PCIR) were a parts per thousand aEuro parts per thousand 30 nT(2) and < 10 nT(2) in the high speed streams proper.
C1 [Echer, E.; Tsurutani, B. T.; Gonzalez, W. D.] Natl Inst Space Res INPE, Sao Jose Dos Campos, SP, Brazil.
[Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kozyra, J. U.] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Echer, E (reprint author), Natl Inst Space Res INPE, Sao Jose Dos Campos, SP, Brazil.
EM ezequiel.echer@gmail.com; bruce.tsurutani@jpl.nasa.gov;
gonzalez@dge.inpe.br; jukozyra@umich.edu
RI Tecnologias espaciai, Inct/I-2415-2013
FU CNPq [PQ-300211/2008-2]; FAPESP [2007/52533-1]; FAPESP agency
[2008/06650-9]; Jet Propulsion Laboratory, California Institute of
Technology; NASA; NSF [0903596]
FX E.E. would like to thank the CNPq (PQ-300211/2008-2) and FAPESP
(2007/52533-1) agencies for their financial support. W.D.G. would like
to thank the FAPESP agency (2008/06650-9) for its financial support.
Portions of this work were performed at the Jet Propulsion Laboratory,
California Institute of Technology under contract with NASA. B.T.T.
thanks INPE for logistical support during his stay in Sao Jose dos
Campos. J.U.K.'s work was supported by NSF under grant 0903596.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD DEC
PY 2011
VL 274
IS 1-2
BP 303
EP 320
DI 10.1007/s11207-011-9739-0
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873ER
UT WOS:000298864400017
ER
PT J
AU Lepping, RP
Wu, CC
Berdichevsky, DB
Szabo, A
AF Lepping, R. P.
Wu, C. -C.
Berdichevsky, D. B.
Szabo, A.
TI Magnetic Clouds at/near the 2007-2009 Solar Minimum: Frequency of
Occurrence and Some Unusual Properties
SO SOLAR PHYSICS
LA English
DT Article
ID GEOMAGNETIC STORMS; INNER HELIOSPHERE; WIND; AU; PARAMETERS; EVOLUTION;
VOYAGER; ORIGIN; ERRORS; FIELDS
AB Magnetic clouds (MCs) have been identified for the period 2007 -aEuro parts per thousand 2009 (at/near the recent solar minimum) from Wind data, then confirmed through MC parameter fitting using a force-free model. A dramatic increase in the frequency of occurrence of these events took place from the two early years of 2007 (with five MCs) and 2008 (one MC) compared to 2009 (12 MCs). This pattern approximately mirrors the occurrence-frequency profile that was observed over a three-year interval 12 years earlier, with eight events in 1995, four in 1996, and 17 in 1997, but decreased overall by a factor of 0.62 in number. However, the average estimated axial field strength [aOE (c)|B (O)|>] taken over all of the 18 events of 2007 -aEuro parts per thousand 2009 (called the "recent period" here) was only 11.0 nT, whereas aOE (c)|B (O)|> for the 29 events of 1995 -aEuro parts per thousand 1997 (called the "earlier period") was 16.5 nT. This 33% average drop in aOE (c)|B (O)|> is more or less consistent with the decreased three-year average interplanetary magnetic field intensity between these two periods, which shows a 23% drop. In the earlier period, the MCs were clearly of mixed types but predominantly of the South-to-North type, whereas those in the recent period are almost exclusively the North-to-South type; this change is consistent with global solar field changes predicted by Bothmer and Rust (Geophys. Monogr. Ser. 99, 139, 1997). As we have argued in earlier work (Lepping and Wu, J. Geophys. Res. 112, A10103, 2007), this change should make it possible to carry out (accurate short-term) magnetic storm forecasting by predicting the latter part of an MC from the earlier part, using a good MC parameter-fitting model with real-time data from a spacecraft at L-1, for example. The recent set's average duration is 15.2 hours, which is a 27% decrease compared to that of the earlier set, which had an average duration of 20.9 hours. In fact, all physical aspects of the recent MC set are shown to drop with respect to the earlier set; e.g., as well as the average internal magnetic field drop, the recent set had a somewhat low average speed of 379 km s(-1) (5% drop), and the average diameter had a 24% drop. Hence, compared to the earlier set, the recent set consists of events that are smaller, slightly slower, and weaker in every respect (and fewer in number), but in a relative sense the two three-year sets have similar frequency-of-occurrence profiles. It is also interesting that the two sets have almost the same average axial inclinations, i.e., axial latitude a parts per thousand 31A degrees (in GSE). These MC characteristics are compared to relevant solar features and their changes. A preliminary assessment of the statistics on possible shocks and pressure pulses upstream of these recent MCs yields the following: About 28% of the MCs, at most, had shocks, and 33% had shocks and/or pressure pulses. These are low values, since typically the percentage of cases with shocks is about 50%, and the percentage with shocks and/or pressure pulses is usually about 75%.
C1 [Lepping, R. P.; Szabo, A.] NASA, Goddard Space Flight Ctr, Heliosphys Sci Div, Greenbelt, MD 20771 USA.
[Wu, C. -C.] USN, Res Lab, Washington, DC USA.
[Berdichevsky, D. B.] Univ Dist Columbia, Dept Elect & Comp Engn, Washington, DC 20008 USA.
RP Lepping, RP (reprint author), NASA, Goddard Space Flight Ctr, Heliosphys Sci Div, Greenbelt, MD 20771 USA.
EM Ronald.P.Lepping@gmail.com
FU NASA [NNG10PB25P]; NRL [N00173-10-1-G021]; NASA LWS [NNH09AM46I]
FX We thank the Wind/MFI and SWE teams for the care they employ in
producing the plasma and field data used for this work, and in
particular we thank Keith Ogilvie, the principal investigator of SWE,
and Franco Mariani of the MFI team for his careful instrument
calibrations. We kindly thank Neil Sheeley, for helpful comments on
aspects of recent solar cycle behavior, and Kan Liou, for computing the
average background magnetic field intensity for the years 1995 - 1997
and 2007 - 2009 that we use for some comparisons. This work was
supported by a NASA program under grant number NNG10PB25P and under NRL
grant number N00173-10-1-G021. CCW was partially supported by the NASA
LWS program under grant number NNH09AM46I.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD DEC
PY 2011
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BP 345
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DI 10.1007/s11207-010-9646-9
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873ER
UT WOS:000298864400019
ER
PT J
AU Emery, BA
Richardson, IG
Evans, DS
Rich, FJ
Wilson, GR
AF Emery, Barbara A.
Richardson, Ian G.
Evans, David S.
Rich, Frederick J.
Wilson, Gordon R.
TI Solar Rotational Periodicities and the Semiannual Variation in the Solar
Wind, Radiation Belt, and Aurora
SO SOLAR PHYSICS
LA English
DT Article
DE Solar cycle; Solar rotation periodicities; Geospace; Aurora; Radiation
belt electron flux; Solar wind; Semiannual periodicity
ID CORONAL MASS EJECTIONS; GEOMAGNETIC-ACTIVITY; SPACED DATA; SPEED; CYCLE;
ELECTRONS; STORMS; PRECIPITATION; EVOLUTION; FEATURES
AB The behavior of a number of solar wind, radiation belt, auroral and geomagnetic parameters is examined during the recent extended solar minimum and previous solar cycles, covering the period from January 1972 to July 2010. This period includes most of the solar minimum between Cycles 23 and 24, which was more extended than recent solar minima, with historically low values of most of these parameters in 2009. Solar rotational periodicities from 5 to 27 days were found from daily averages over 81 days for the parameters. There were very strong 9-day periodicities in many variables in 2005 -aEuro parts per thousand 2008, triggered by recurring corotating high-speed streams (HSS). All rotational amplitudes were relatively large in the descending and early minimum phases of the solar cycle, when HSS are the predominant solar wind structures. There were minima in the amplitudes of all solar rotational periodicities near the end of each solar minimum, as well as at the start of the reversal of the solar magnetic field polarity at solar maximum (similar to aEuro parts per thousand 1980, similar to aEuro parts per thousand 1990, and similar to aEuro parts per thousand 2001) when the occurrence frequency of HSS is relatively low. Semiannual equinoctial periodicities, which were relatively strong in the 1995 -aEuro parts per thousand 1997 solar minimum, were found to be primarily the result of the changing amplitudes of the 13.5- and 27-day periodicities, where 13.5-day amplitudes were better correlated with heliospheric daily observations and 27-day amplitudes correlated better with Earth-based daily observations. The equinoctial rotational amplitudes of the Earth-based parameters were probably enhanced by a combination of the Russell-McPherron effect and a reduction in the solar wind-magnetosphere coupling efficiency during solstices. The rotational amplitudes were cross-correlated with each other, where the 27-day amplitudes showed some of the weakest cross-correlations. The rotational amplitudes of the > 2 MeV radiation belt electron number fluxes were progressively weaker from 27- to 5-day periods, showing that processes in the magnetosphere act as a low-pass filter between the solar wind and the radiation belt. The A (p)/K (p) magnetic currents observed at subauroral latitudes are sensitive to proton auroral precipitation, especially for 9-day and shorter periods, while the A (p)/K (p) currents are governed by electron auroral precipitation for 13.5- and 27-day periodicities.
C1 [Emery, Barbara A.] HAO NCAR, Boulder, CO 80301 USA.
[Richardson, Ian G.] Univ Maryland, GSFC, College Pk, MD 20742 USA.
[Richardson, Ian G.] Univ Maryland, CRESST Dept Astron, College Pk, MD 20742 USA.
[Evans, David S.] SWPC NOAA, Boulder, CO 80305 USA.
[Rich, Frederick J.] LL MIT, Lexington, MA 02420 USA.
[Wilson, Gordon R.] AFRL RVBXP, Kirtland Afb, NM 87117 USA.
RP Emery, BA (reprint author), HAO NCAR, 3080 Ctr Green, Boulder, CO 80301 USA.
EM emery@ucar.edu
OI Richardson, Ian/0000-0002-3855-3634
FU National Science Foundation (NSF); National Science Foundation at the
High Altitude Observatory within the National Center for Atmospheric
Research; National Aeronautics and Space Administration (NASA) at the
Goddard Space Flight Center
FX The original and the intercalibrated DMSP and NOAA satellite hemispheric
power estimates were taken from the Coupling, Energetics, and Dynamics
of Atmospheric Regions (CEDAR) Database, which is supported by the
National Science Foundation (NSF). The Air Force Research Laboratory
Auroral Boundary Index (ABI) was provided by the USAF Research
Laboratory, Hanscom AFB, MA via the CEDAR Database. The hourly solar
wind plasma and IMF data were taken from the OMNI-2 collection from the
Space Physics Data Facility at the Goddard Space Flight Center managed
by Dr. Natalia Papitashvili. B.A.E. is supported by the National Science
Foundation at the High Altitude Observatory within the National Center
for Atmospheric Research. I.G.R. is supported by the National
Aeronautics and Space Administration (NASA) at the Goddard Space Flight
Center.
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JI Sol. Phys.
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SC Astronomy & Astrophysics
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UT WOS:000298864400022
ER
PT J
AU Russell, CT
Raymond, CA
AF Russell, C. T.
Raymond, C. A.
TI The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres Foreword
SO SPACE SCIENCE REVIEWS
LA English
DT Editorial Material
C1 [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Russell, CT (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
EM ctrussel@igpp.ucla.edu
RI Russell, Christopher/E-7745-2012
OI Russell, Christopher/0000-0003-1639-8298
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J9 SPACE SCI REV
JI Space Sci. Rev.
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SC Astronomy & Astrophysics
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UT WOS:000299002100001
ER
PT J
AU Russell, CT
Raymond, CA
AF Russell, C. T.
Raymond, C. A.
TI The Dawn Mission to Vesta and Ceres
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Dawn mission; Vesta; Ceres; Asteroid belt
AB The Dawn mission journeys to the center of the main asteroid belt to orbit and explore the two most massive main belt asteroids, Vesta and Ceres. Dawn aims to increase our understanding not just of the present state of these two bodies, but also of the conditions during the time of their formation. It attempts this through achieving a set of measurement objectives in which the physical properties of these asteroids such as mass, slopes, size, density, and spin state are accurately determined, and in which the mineralogical and elemental composition of the surface and near-surface material are probed. Dawn employs ion propulsion technology to enable a modestly-sized launcher to start a moderately-sized spacecraft on its journey, to not only reach the two massive asteroids but also to orbit them, descending to near the surface. Unlike most orbital missions, the initial (Vesta) phase must be completed with sufficient reserves and within a time window that later allows Dawn to explore Ceres. Dawn carries a redundant framing camera, a visible and near-IR spectrometer, a gamma ray and neutron spectrometer, and achieves high-accuracy radiometric and optical navigation to enable gravity field determination. The spacecraft was developed by Orbital Sciences Corporation under the management of the Jet Propulsion Laboratory for the National Aeronautics and Space Administration. Dawn is a Principal Investigator-led mission of the Discovery Program. The PI institution, the University of California, Los Angeles, manages directly the science team, the Dawn Science Center, and the Education and Public Outreach program.
C1 [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Russell, CT (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
EM ctrussel@igpp.ucla.edu
RI Russell, Christopher/E-7745-2012
OI Russell, Christopher/0000-0003-1639-8298
FU National Aeronautics and Space Administration [NNM05AA86C]
FX The preparation of this report was supported by the National Aeronautics
and Space Administration under contract NNM05AA86C. A portion of the
work was carried out at the Jet Propulsion Laboratory.; Those with whom
we worked most closely include personnel from NASA's Lewis Research
Center (now Glenn), from JPL, from TRW, Orbital and their
subcontractors, from NASA Headquarters, from the Discovery Program
Office at NASA Marshall Space Flight Center, from Los Alamos, from the
Max Planck Institute, from INAF, from DLR, from ASI and all the
organizations supporting the members of the science teams deserve much
thanks. We are especially grateful to the Project Managers at JPL and at
the various contractors and subcontractors who were so dedicated to
making Dawn a success that they put their jobs on the line to ensure it
would be. Finally, we thank Robert Mase who has led the project during
its operational phase since shortly after launch.
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JI Space Sci. Rev.
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BP 3
EP 23
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SC Astronomy & Astrophysics
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UT WOS:000299002100002
ER
PT J
AU McCord, TB
Castillo-Rogez, J
Rivkin, A
AF McCord, Thomas B.
Castillo-Rogez, Julie
Rivkin, Andy
TI Ceres: Its Origin, Evolution and Structure and Dawn's Potential
Contribution
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Dawn; Ceres; Evolution of ice-silicate bodies
ID THERMAL EVOLUTION; PARENT BODIES; ASTEROID BELT; LIQUID WATER; 2 PALLAS;
SURFACE; ORGANICS; OBJECTS; MOON; MASS
AB Ceres appears likely to be differentiated and to have experienced planetary evolution processes. This conclusion is based on current geophysical observations and thermodynamic modeling of Ceres' evolution. This makes Ceres similar to a small planet, and in fact it is thought to represent a class of objects from which the inner planets formed. Verification of Ceres' state and understanding of the many steps in achieving it remains a major goal. The Dawn spacecraft and its instrument package are on a mission to observe Ceres from orbit. Observations and potential results are suggested here, based on number of science questions.
C1 [McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Castillo-Rogez, Julie] Calif Inst Planetol, Jet Prop Lab, Pasadena, CA USA.
[Rivkin, Andy] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP McCord, TB (reprint author), Bear Fight Inst, 22 Fiddlers Rd, Winthrop, WA 98862 USA.
EM tmccord@bearfightinstitute.com
RI Rivkin, Andrew/B-7744-2016
OI Rivkin, Andrew/0000-0002-9939-9976
FU NASA
FX We thank J.-Y. Li for helpful comments on an early draft and two
anonymous reviewers for their helpful comments. This research was
partially supported by the NASA Dawn Project under contract from UCLA.
Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract to NASA. All rights
reserved. Government sponsorship acknowledged.
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JI Space Sci. Rev.
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SC Astronomy & Astrophysics
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UT WOS:000299002100005
ER
PT J
AU Zuber, MT
McSween, HY
Binzel, RP
Elkins-Tanton, LT
Konopliv, AS
Pieters, CM
Smith, DE
AF Zuber, Maria T.
McSween, Harry Y., Jr.
Binzel, Richard P.
Elkins-Tanton, Linda T.
Konopliv, Alexander S.
Pieters, Carle M.
Smith, David E.
TI Origin, Internal Structure and Evolution of 4 Vesta
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Vesta; Asteroid; Crust; Mantle; Core; Evolution; Impact
ID EUCRITE PARENT BODY; EARLY SOLAR-SYSTEM; CIRCUMSTELLAR DISKS;
TERRESTRIAL PLANETS; ASTEROID-4 VESTA; GLOBAL SOLUTION; CORE FORMATION;
MAGMA OCEAN; DIOGENITES; METEORITES
AB Asteroid 4 Vesta is the only preserved intact example of a large, differentiated protoplanet like those believed to be the building blocks of terrestrial planet accretion. Vesta accreted rapidly from the solar nebula in the inner asteroid belt and likely melted due to heat released due to the decay of (26)Al. Analyses of meteorites from the howardite-eucrite-diogenite (HED) suite, which have been both spectroscopically and dynamically linked to Vesta, lead to a model of the asteroid with a basaltic crust that overlies a depleted peridotitic mantle and an iron core. Vesta's crust may become more mafic with depth and might have been intruded by plutons arising from mantle melting. Constraints on the asteroid's moments of inertia from the long-wavelength gravity field, pole position and rotation, informed by bulk composition estimates, allow tradeoffs between mantle density and core size; cores of up to half the planetary radius can be consistent with plausible mantle compositions. The asteroid's present surface is expected to consist of widespread volcanic terrain, modified extensively by impacts that exposed the underlying crust or possibly the mantle. Hemispheric heterogeneity has been observed by poorly resolved imaging of the surface that suggests the possibility of a physiographic dichotomy as occurs on other terrestrial planets. Vesta might have had an early magma ocean but details of the early thermal structure are far from clear owing to model uncertainties and paradoxical observations from the HEDs. Petrological analysis of the eucrites coupled with thermal evolution modeling recognizes two possible mechanisms of silicate-metal differentiation leading to the formation of the basaltic achondrites: equilibrium partial melting or crystallization of residual liquid from the cooling magma ocean. A firmer understanding the plethora of complex physical and chemical processes that contribute to melting and crystallization will ultimately be required to distinguish among these possibilities. The most prominent physiographic feature on Vesta is the massive south polar basin, whose formation likely re-oriented the body axis of the asteroid's rotation. The large impact represents the likely major mechanism of ejection of fragments that became the HEDs. Observations from the Dawn mission hold the promise of revolutionizing our understanding of 4 Vesta, and by extension, the nature of collisional, melting and differentiation processes in the nascent solar system.
C1 [Zuber, Maria T.; Binzel, Richard P.; Elkins-Tanton, Linda T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[McSween, Harry Y., Jr.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Konopliv, Alexander S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
RP Zuber, MT (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
EM zuber@mit.edu
RI Elkins-Tanton, Linda/C-5508-2008
OI Elkins-Tanton, Linda/0000-0003-4008-1098
FU NASA [NNM05AA86C]
FX The Dawn mission is supported by the NASA Discovery Program under
contract NNM05AA86C.
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JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 77
EP 93
DI 10.1007/s11214-011-9806-8
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
UT WOS:000299002100006
ER
PT J
AU Rivkin, AS
Li, JY
Milliken, RE
Lim, LF
Lovell, AJ
Schmidt, BE
McFadden, LA
Cohen, BA
AF Rivkin, Andrew S.
Li, Jian-Yang
Milliken, Ralph E.
Lim, Lucy F.
Lovell, Amy J.
Schmidt, Britney E.
McFadden, Lucy A.
Cohen, Barbara A.
TI The Surface Composition of Ceres
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Asteroids; Dwarf planets; Solar system; Spectroscopy; Dawn mission;
Composition
ID MAIN-BELT ASTEROIDS; SPECTRAL IRRADIANCE CALIBRATION; CARLSBERG MERIDIAN
CIRCLE; HUBBLE-SPACE-TELESCOPE; MU-M SPECTRA; MINOR PLANETS;
POLARIMETRIC OBSERVATIONS; CARBONACEOUS CHONDRITES; PHOTOMETRIC
ANALYSIS; SPECTROSCOPIC SURVEY
AB Our understanding of the composition of Ceres is driven by remote sensing of its surface. We review spectral observations of Ceres over wavelengths from the ultraviolet to the radio, as well as non-spectral data such as thermal inertia, photometric properties, radar experiments, and surface variability. We also discuss the closest likely meteorite analogs to Ceres and consider the likelihood that material from Ceres could be delivered to Earth.
C1 [Rivkin, Andrew S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Li, Jian-Yang; McFadden, Lucy A.] Univ Maryland, College Pk, MD 20742 USA.
[Milliken, Ralph E.] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Lim, Lucy F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lovell, Amy J.] Agnes Scott Coll, Atlanta, GA USA.
[Schmidt, Britney E.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Cohen, Barbara A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Rivkin, AS (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
EM andrew.rivkin@jhuapl.edu
RI Lim, Lucy/C-9557-2012; McFadden, Lucy-Ann/I-4902-2013; Rivkin,
Andrew/B-7744-2016;
OI Lim, Lucy/0000-0002-9696-9654; McFadden, Lucy-Ann/0000-0002-0537-9975;
Rivkin, Andrew/0000-0002-9939-9976; Schmidt, Britney/0000-0001-7376-8510
FU NASA
FX ASR acknowledges support from the NASA Planetary Astronomy program.
Thanks, whether direct, belated, or vicarious, to the original observers
and telescope operators whose data are reviewed here. Thanks to Bobby
Bus for contributing some of his data. Helpful reviews by Alberto
Cellino and an anonymous reviewer improved the manuscript to its current
state. Numerous helpful discussions with dozens of colleagues centering
on Ceres have occurred over the past several months due to the NRC
Planetary Science Decadal Survey effort, which indirectly and directly
improved our all-around understanding of Ceres.
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SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 95
EP 116
DI 10.1007/s11214-010-9677-4
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
UT WOS:000299002100007
ER
PT J
AU Pieters, CM
McFadden, LA
Prettyman, T
De Sanctis, MC
McCord, TB
Hiroi, T
Klima, R
Li, JY
Jaumann, R
AF Pieters, Carle M.
McFadden, Lucy A.
Prettyman, Thomas
De Sanctis, M. Cristina
McCord, Thomas B.
Hiroi, Takahiro
Klima, Rachel
Li, Jian-Yang
Jaumann, Ralf
TI Surface Composition of Vesta: Issues and Integrated Approach
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Vesta composition; Dawn mission; Great South Crater; Space weathering;
Volatiles on asteroids
ID POLAR HYDROGEN DEPOSITS; NEAR-EARTH ASTEROIDS; ORDINARY CHONDRITE; DAWN
MISSION; LUNAR POLES; PARENT BODY; REFLECTANCE SPECTROSCOPY;
SPATIAL-DISTRIBUTION; SPECTRAL PROPERTIES; BASALTIC ASTEROIDS
AB The instruments on the Dawn spacecraft are exceptionally well suited to characterize and map the surface composition of Vesta in an integrated manner. These include a framing camera with multispectral capabilities, a high spectral resolution near-infrared imaging spectrometer, and a gamma-ray and neutron spectrometer. Three examples of issues addressed at Vesta are: (1) What is the composition of Vesta's interior and differentiation state as exposed by the Great South Crater? (2) How has space weathering affected Vesta, both globally and at a local scale? and (3) Are volatiles or hydrated material present on Vesta's surface? We predict that Dawn finds many surprises, such as an olivine-bearing mantle exposed near the south-pole, a weakly or un-weathered surface that has been relatively recently resurfaced, and a very thin layer of surficial volatiles derived from interaction with the solar wind.
C1 [Pieters, Carle M.; Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Prettyman, Thomas] Planetary Sci Inst, Tucson, AZ 85719 USA.
[De Sanctis, M. Cristina] Ist Astrofis Spaziale & Fis Cosm, INAF, Area Ric Tor Vergata, I-00133 Rome, Italy.
[McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Klima, Rachel] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Jaumann, Ralf] Deutsch Zentrum Fuer Luft & Raumfahrt, Inst Planetary Res, Berlin, Germany.
RP Pieters, CM (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
EM Carle_Pieters@brown.edu
RI Klima, Rachel/H-9383-2012; McFadden, Lucy-Ann/I-4902-2013; De Sanctis,
Maria Cristina/G-5232-2013;
OI Klima, Rachel/0000-0002-9151-6429; McFadden,
Lucy-Ann/0000-0002-0537-9975; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Prettyman, Thomas/0000-0003-0072-2831
FU NASA [NNM05AA86C, 2090 S JB693]
FX NASA support for this work is greatly appreciated, including NASA
contract NNM05AA86C, subcontract #2090 S JB693. We gratefully
acknowledge the kind permission of N. Moskovitz to include some of his
V-type asteroid data in this overview. Reviews by C. R. Chapman and an
anonymous reviewer were quite helpful and appreciated.
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SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 117
EP 139
DI 10.1007/s11214-011-9809-5
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
UT WOS:000299002100008
ER
PT J
AU McSween, HY
Mittlefehldt, DW
Beck, AW
Mayne, RG
McCoy, TJ
AF McSween, Harry Y., Jr.
Mittlefehldt, David W.
Beck, Andrew W.
Mayne, Rhiannon G.
McCoy, Timothy J.
TI HED Meteorites and Their Relationship to the Geology of Vesta and the
Dawn Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Meteorites; Vesta; Asteroid; Eucrite; Diogenite; Howardite
ID EUCRITE PARENT BODY; EARLY SOLAR-SYSTEM; ASTEROID 4 VESTA;
ORTHO-PYROXENE; BASALTIC METEORITES; MN-53-CR-53 SYSTEMATICS; DIOGENITE
METEORITES; THERMAL METAMORPHISM; ISOTOPE SYSTEMATICS; MARTIAN
METEORITES
AB Howardite-eucrite-diogenite (HED) meteorites, thought to be derived from 4 Vesta, provide the best sampling available for any differentiated asteroid. However, deviations in oxygen isotopic composition from a common mass-fractionation line suggest that a few eucrite-like meteorites are from other bodies, or that Vesta was not completely homogenized during differentiation. The petrology and geochemistry of HEDs provide insights into igneous processes that produced a crust composed of basalts, gabbros, and ultramafic cumulate rocks. Although most HED magmas were fractionated, it is unresolved whether some eucrites may have been primary melts. The geochemistry of HEDs indicates that bulk Vesta is depleted in volatile elements and is relatively reduced, but has chondritic refractory element abundances. The compositions of HEDs may favor a magma ocean model, but inconsistencies remain. Geochronology indicates that Vesta accreted and differentiated within the first several million years of solar system history, that magmatism continued over a span of similar to 10 Myr, and that its thermal history extended for perhaps 100 Myr. The protracted cooling history is probably responsible for thermal metamorphism of most HEDs. Impact chronology indicates that Vesta experienced many significant collisions, including during the late heavy bombardment. The age of the huge south pole crater is controversial, but it probably ejected Vestoids and many HEDs. Continued impacts produced a regolith composed of eucrite and diogenite fragments containing only minor exotic materials. HED meteorites serve as ground truth for orbital spectroscopic and chemical analyses by the Dawn spacecraft, and their properties are critical for instrument calibration and interpretation of Vesta's geologic history.
C1 [McSween, Harry Y., Jr.; Beck, Andrew W.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[McSween, Harry Y., Jr.; Beck, Andrew W.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Mittlefehldt, David W.] NASA, Astromat Res Off, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Mayne, Rhiannon G.] Texas Christian Univ, Dept Geol, Ft Worth, TX 76129 USA.
[McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20546 USA.
RP McSween, HY (reprint author), Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
EM mcsween@utk.edu
RI Beck, Andrew/J-7215-2015
OI Beck, Andrew/0000-0003-4455-2299
FU NASA Cosmochemistry [NNG06GG36G, RTOP 344-31-10-18, NNG06GF56G]
FX We acknowledge thoughtful reviews by P. Warren and an anonymous
reviewer. This work was partly supported by NASA Cosmochemistry grants
NNG06GG36G (HYM), RTOP 344-31-10-18 (DWM), and NNG06GF56G (TJM).
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SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 141
EP 174
DI 10.1007/s11214-010-9637-z
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
UT WOS:000299002100009
ER
PT J
AU Thomas, VC
Makowski, JM
Brown, GM
McCarthy, JF
Bruno, D
Cardoso, JC
Chiville, WM
Meyer, TF
Nelson, KE
Pavri, BE
Termohlen, DA
Violet, MD
Williams, JB
AF Thomas, Valerie C.
Makowski, Joseph M.
Brown, G. Mark
McCarthy, John F.
Bruno, Dominick
Cardoso, J. Christopher
Chiville, W. Michael
Meyer, Thomas F.
Nelson, Kenneth E.
Pavri, Betina E.
Termohlen, David A.
Violet, Michael D.
Williams, Jeffrey B.
TI The Dawn Spacecraft
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE The Orbital-JPL partnership; Early spacecraft concept evolution;
Spacecraft design drivers
AB The Dawn spacecraft is designed to travel to and operate in orbit around the two largest main belt asteroids, Vesta and Ceres. Developed to meet a ten-year life and fully redundant, the spacecraft accommodates an ion propulsion system, including three ion engines and xenon propellant tank, utilizes large solar arrays to power the engines, carries the science instrument payload, and hosts the hardware and software required to successfully collect and transmit the scientific data back to Earth. The launch of the Dawn spacecraft in September 2007 from Cape Canaveral Air Force Station was the culmination of nearly five years of design, development, integration and testing of this unique system, one of the very few scientific spacecraft to rely on ion propulsion. The Dawn spacecraft arrived at its first destination, Vesta, in July 2011, where it will conduct science operations for twelve months before departing for Ceres.
C1 [Thomas, Valerie C.; Brown, G. Mark; Pavri, Betina E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Makowski, Joseph M.; McCarthy, John F.; Bruno, Dominick; Cardoso, J. Christopher; Chiville, W. Michael; Meyer, Thomas F.; Nelson, Kenneth E.; Termohlen, David A.; Violet, Michael D.; Williams, Jeffrey B.] Orbital Sci Corp, Dulles, VA 20166 USA.
RP Thomas, VC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM valerie.c.thomas@jpl.nasa.gov
FU JPL, Orbital Sciences Corporation
FX The authors wish to express their appreciation all the individuals at
JPL, Orbital Sciences Corporation and their many subcontractors, whose
hard work and dedication contributed to getting the Dawn spacecraft off
the ground and on its voyage. The work 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 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
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BP 175
EP 249
DI 10.1007/s11214-011-9852-2
PG 75
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
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UT WOS:000299002100010
ER
PT J
AU Brophy, J
AF Brophy, John
TI The Dawn Ion Propulsion System
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Dawn; Ion propulsion; Electric propulsion; SEP
AB Dawn's ion propulsion system (IPS) is the most advanced propulsion system ever built for a deep-space mission. Aside from the Mars gravity assist it provides all of the post-launch Delta V required for the mission including the heliocentric transfer to Vesta, orbit capture at Vesta, transfer to various Vesta science orbits, escape from Vesta, the heliocentric transfer to Ceres, orbit capture at Ceres, and transfer to the different Ceres science orbits. The ion propulsion system provides a total Delta V of nearly 11 km/s, comparable to the Delta V provided by the 3-stage launch vehicle, and a total impulse of 1.2x10(7) N s.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Brophy, J (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM john.r.brophy@jpl.nasa.gov
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SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 251
EP 261
DI 10.1007/s11214-011-9848-y
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
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UT WOS:000299002100011
ER
PT J
AU Konopliv, AS
Asmar, SW
Bills, BG
Mastrodemos, N
Park, RS
Raymond, CA
Smith, DE
Zuber, MT
AF Konopliv, A. S.
Asmar, S. W.
Bills, B. G.
Mastrodemos, N.
Park, R. S.
Raymond, C. A.
Smith, D. E.
Zuber, M. T.
TI The Dawn Gravity Investigation at Vesta and Ceres
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Dawn; Vesta; Ceres; Gravity; Geophysics
ID INTERNAL STRUCTURE; INTERIOR STRUCTURE; DOPPLER TRACKING; GLOBAL
SOLUTION; KORONIS FAMILY; ASTEROIDS; EARTH; DYNAMICS; ROTATION; INERTIA
AB The objective of the Dawn gravity investigation is to use high precision X-band Doppler tracking and landmark tracking from optical images to measure the gravity fields of Vesta and Ceres to a half-wavelength surface resolution better than 90-km and 300-km, respectively. Depending on the Doppler tracking assumptions, the gravity field will be determined to somewhere between harmonic degrees 15 and 25 for Vesta and about degree 10 for Ceres. The gravity fields together with shape models determined from Dawn's framing camera constrain models of the interior from the core to the crust. The gravity field is determined jointly with the spin pole location. The second degree harmonics together with assumptions on obliquity or hydrostatic equilibrium may determine the moments of inertia.
C1 [Konopliv, A. S.; Asmar, S. W.; Bills, B. G.; Mastrodemos, N.; Park, R. S.; Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Smith, D. E.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Konopliv, AS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alex.konopliv@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration
FX Bob Werner provided polyhedral software and assistance for the
gravitational modeling of multilayered Vesta shape models. The research
described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
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JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 461
EP 486
DI 10.1007/s11214-011-9794-8
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
UT WOS:000299002100015
ER
PT J
AU Raymond, CA
Jaumann, R
Nathues, A
Sierks, H
Roatsch, T
Preusker, F
Scholten, F
Gaskell, RW
Jorda, L
Keller, HU
Zuber, MT
Smith, DE
Mastrodemos, N
Mottola, S
AF Raymond, C. A.
Jaumann, R.
Nathues, A.
Sierks, H.
Roatsch, T.
Preusker, F.
Scholten, F.
Gaskell, R. W.
Jorda, L.
Keller, H-U.
Zuber, M. T.
Smith, D. E.
Mastrodemos, N.
Mottola, S.
TI The Dawn Topography Investigation
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Vesta; Ceres; Dawn; Asteroid topography
ID EXPRESS HRSC DATA; MARS-EXPRESS; VESTA; MISSION; CERES; SHAPE;
HETEROGENEITY; INSTRUMENT; IMAGES
AB The objective of the Dawn topography investigation is to derive the detailed shapes of 4 Vesta and 1 Ceres in order to create orthorectified image mosaics for geologic interpretation, as well as to study the asteroids' landforms, interior structure, and the processes that have modified their surfaces over geologic time. In this paper we describe our approaches for producing shape models, plans for acquiring the needed image data for Vesta, and the results of a numerical simulation of the Vesta mapping campaign that quantify the expected accuracy of our results. Multi-angle images obtained by Dawn's framing camera will be used to create topographic models with 100 m/pixel horizontal resolution and 10 m height accuracy at Vesta, and 200 m/pixel horizontal resolution and 20 m height accuracy at Ceres. Two different techniques, stereophotogrammetry and stereophotoclinometry, are employed to model the shape; these models will be merged with the asteroidal gravity fields obtained by Dawn to produce geodetically controlled topographic models for each body. The resulting digital topography models, together with the gravity data, will reveal the tectonic, volcanic and impact history of Vesta, and enable co-registration of data sets to determine Vesta's geologic history. At Ceres, the topography will likely reveal much about processes of surface modification as well as the internal structure and evolution of this dwarf planet.
C1 [Raymond, C. A.; Mastrodemos, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jaumann, R.; Roatsch, T.; Preusker, F.; Scholten, F.; Mottola, S.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetary Res, Berlin, Germany.
[Nathues, A.; Sierks, H.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Gaskell, R. W.] Planetary Sci Inst, Tucson, AZ USA.
[Jorda, L.] Lab Astrophys Marseille, Marseille, France.
[Keller, H-U.] Univ Berlin, Dept Earth Sci Remote Sensing Earth & Planets, Berlin, Germany.
[Zuber, M. T.; Smith, D. E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Smith, D. E.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Raymond, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM carol.a.raymond@jpl.nasa.gov
FU NASA
FX The authors are grateful for support of the Virtual Vesta analysis by
the Dawn project team, and for the comments of two anonymous reviewers,
which improved the paper. A portion of this work was performed at the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
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JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
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BP 487
EP 510
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SC Astronomy & Astrophysics
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UT WOS:000299002100016
ER
PT J
AU Polanskey, CA
Joy, SP
Raymond, CA
AF Polanskey, C. A.
Joy, S. P.
Raymond, C. A.
TI Dawn Science Planning, Operations and Archiving
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Vesta; Dawn; Asteroid mission; Science mission operations
AB The Dawn science operations team has designed the Vesta mission within the constraints of a low-cost Discovery mission, and will apply the same methodology to the Ceres mission. The design employs proactive mapping mission strategies and tactics such as functional redundancy, adaptability to trajectory uncertainties, and easy sequence updates to deliver reliable and robust sequences. Planning tools include the Science Opportunity Analyzer and other multi-mission tools, and the Science time-ordered listings. Science operations are conducted jointly by the Science Operations Support Team at the Jet Propulsion Laboratory (JPL) and the Dawn Science Center at the University of California, Los Angeles (UCLA). The UCLA Dawn Science Center has primary responsibility for data archiving while the JPL team has primary responsibility for spacecraft and instrument operations. Constraints and uncertainties in the planning and sequencing environment are described, and then details of the science plan are presented for each mission sub-phase. The plans indicate that Dawn has a high probability of meeting its science objectives and requirements within the imposed constraints.
C1 [Polanskey, C. A.; Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Joy, S. P.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Polanskey, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Carol.Polanskey@jpl.nasa.gov
FU NASA
FX The authors wish to acknowledge Tony Vanelli and Brett Smith for
development and implementation of the ACN pointing mode that enabled the
observation strategy as conceived in the science plan. We thank Joe Mafi
for his contribution to the development of the DSC tools and the DSDb.
We also thank the SOA development team: Taifun O'Reilly, Barbara
Streiffert, Jeff Bytof, Ning Liu, Robert Witoff and Jay Torres for their
support of the Dawn adaptation of SOA. The success of this endeavor also
depended on the support of the Dawn flight operations team. A portion of
this work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA.
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SC Astronomy & Astrophysics
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UT WOS:000299002100017
ER
PT J
AU Mcfadden, LA
Wise, J
Ristvey, JD
Cobb, W
AF Mcfadden, L. A.
Wise, J.
Ristvey, J. D., Jr.
Cobb, W.
TI The Education and Public Outreach Program for NASA's Dawn Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Science; Technology; Engineering and mathematical education; Public
outreach; Dawn mission
AB The Dawn mission's Education and Public Outreach (E/PO) program takes advantage of the length of the mission, an effort to maintain level funding, and the exceptional support of the science and engineering teams to create formal and informal educational materials that bring STEM content and modes of thinking to students of all ages. With materials that are based on researched pedagogical principles and aligned with science education standards, Dawn weaves together many aspects of the mission to engage students, teachers, and the general public. E/PO tells the story of the discovery of the asteroid belt, uncovers principles of physics behind the ion propulsion that powers the spacecraft, and explains what we can learn from the instrumentation and how the mission's results will expand our understanding of the origins of the solar system. In this way, we not only educate and inform, we build anticipation and expectation in the general public for the spacecraft's arrival at Vesta in 2011 and three years later at Ceres. This chapter discusses the organization, strategies, formative assessment and dissemination of these materials and activities, and includes a section on lessons learned.
C1 [Mcfadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wise, J.] New Rd Sch, Santa Monica, CA 90404 USA.
[Ristvey, J. D., Jr.; Cobb, W.] Midcontinent Res Educ & Learning, Denver, CO 80237 USA.
RP Mcfadden, LA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lucy.mcfadden@nasa.gov
RI McFadden, Lucy-Ann/I-4902-2013
OI McFadden, Lucy-Ann/0000-0002-0537-9975
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UT WOS:000299002100018
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PT J
AU Mielke, RE
Robinson, KJ
White, LM
McGlynn, SE
McEachern, K
Bhartia, R
Kanik, I
Russell, MJ
AF Mielke, Randall E.
Robinson, Kirtland J.
White, Lauren M.
McGlynn, Shawn E.
McEachern, Kavan
Bhartia, Rohit
Kanik, Isik
Russell, Michael J.
TI Iron-Sulfide-Bearing Chimneys as Potential Catalytic Energy Traps at
Life's Emergence
SO ASTROBIOLOGY
LA English
DT Article
DE Dendrites; Framboids; Greigite; Hydrothermal chimneys; Mackinawite;
Origin of life
ID CITY HYDROTHERMAL FIELD; MID-ATLANTIC RIDGE; AMINO-ACIDS;
AQUEOUS-SOLUTIONS; SEA-FLOOR; SULFUR CLUSTERS; CARBON FIXATION;
OXIDATION-STATE; VENT FIELD; EVOLUTION
AB The concept that life emerged where alkaline hydrogen-bearing submarine hot springs exhaled into the most ancient acidulous ocean was used as a working hypothesis to investigate the nature of precipitate membranes. Alkaline solutions at 25-70 degrees C and pH between 8 and 12, bearing HS(-) +/- silicate, were injected slowly into visi-jars containing ferrous chloride to partially simulate the early ocean on this or any other wet and icy, geologically active rocky world. Dependent on pH and sulfide content, fine tubular chimneys and geodal bubbles were generated with semipermeable walls 4-100 mu m thick that comprised radial platelets of nanometric mackinawite [FeS] +/- ferrous hydroxide [similar to Fe(OH)(2)], accompanied by silica and, at the higher temperature, greigite [Fe(3)S(4)]. Within the chimney walls, these platelets define a myriad of micropores. The interior walls of the chimneys host iron sulfide framboids, while, in cases where the alkaline solution has a pH>11 or relatively low sulfide content, their exteriors exhibit radial flanges with a spacing of similar to 4 mu m that comprise microdendrites of ferrous hydroxide. We speculate that this pattern results from outward and inward radial flow through the chimney walls. The outer Fe(OH)(2) flanges perhaps precipitate where the highly alkaline flow meets the ambient ferrous iron-bearing fluid, while the intervening troughs signal where the acidulous iron-bearing solutions could gain access to the sulfidic and alkaline interior of the chimneys, thereby leading to the precipitation of the framboids. Addition of soluble pentameric peptides enhances membrane durability and accentuates the crenulations on the chimney exteriors. These dynamic patterns may have implications for acid-base catalysis and the natural proton motive force acting through the matrix of the porous inorganic membrane. Thus, within such membranes, steep redox and pH gradients would bear across the nanometric platelets and separate the two counter-flowing solutions, a condition that may have led to the onset of an autotrophic metabolism through the reduction of carbon dioxide.
C1 [Kanik, Isik; Russell, Michael J.] CALTECH, Jet Prop Lab, Sect 3225, Pasadena, CA 91109 USA.
[McGlynn, Shawn E.] Montana State Univ, NASA NAI Astrobiol Biogeocatalysis Res Ctr, Bozeman, MT 59717 USA.
RP Kanik, I (reprint author), CALTECH, Jet Prop Lab, Sect 3225, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM isik.kanik@jpl.nasa.gov; mrussell@jpl.nasa.gov
FU National Aeronautics and Space Administration New York Space Grant
Consortium; ConvEne IGERT [NSF-DGE 0801627]; Marine Biological
Laboratories NASA Planetary Biology; NSF IGERT, MSU Program in
Geobiological Systems [DGE 0654336]; NASA Astrobiology Institute-Montana
State University Astrobiology Biogeocatalysis Research Center
[NNA08CN85A]; NASA [NNH06ZDA001N]; NASA Astrobiology Institute (Icy
Worlds)
FX We thank Bill Abbey, Mathieu Choukroun, James Gleixner, and Richard Kidd
for help in the laboratory. For discussions we are grateful to Wolfgang
Nitschke, Laszlo Roszlo, and Professor Galen Stucky, as well as Laurie
Barge, Elbert Branscomb, and Eugenio Simoncini, members of the
NAI-sponsored Thermodynamics Disequilibrium and Evolution Focus Group.
K. R. thanks the National Aeronautics and Space Administration New York
Space Grant Consortium for financial sponsorship. L. W. is supported by
the ConvEne IGERT Program (NSF-DGE 0801627). S. E. M. was supported by
the Marine Biological Laboratories NASA Planetary Biology Internship
Program, an NSF IGERT Fellowship by the MSU Program in Geobiological
Systems (DGE 0654336) and acknowledges the NASA Astrobiology
Institute-Montana State University Astrobiology Biogeocatalysis Research
Center (NNA08CN85A). The research described in this publication was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration, with support by NASA Exobiology and Evolutionary Biology
award (NNH06ZDA001N) and supported by the NASA Astrobiology Institute
(Icy Worlds).
NR 145
TC 29
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U1 5
U2 52
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 DEC
PY 2011
VL 11
IS 10
BP 933
EP 950
DI 10.1089/ast.2011.0667
PG 18
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 865YA
UT WOS:000298345600001
PM 22111762
ER
PT J
AU Nicholson, WL
Ricco, AJ
Agasid, E
Beasley, C
Diaz-Aguado, M
Ehrenfreund, P
Friedericks, C
Ghassemieh, S
Henschke, M
Hines, JW
Kitts, C
Luzzi, E
Ly, D
Mai, N
Mancinelli, R
McIntyre, M
Minelli, G
Neumann, M
Parra, M
Piccini, M
Rasay, RM
Ricks, R
Santos, O
Schooley, A
Squires, D
Timucin, L
Yost, B
Young, A
AF Nicholson, Wayne L.
Ricco, Antonio J.
Agasid, Elwood
Beasley, Christopher
Diaz-Aguado, Millan
Ehrenfreund, Pascale
Friedericks, Charles
Ghassemieh, Shakib
Henschke, Michael
Hines, John W.
Kitts, Christopher
Luzzi, Ed
Ly, Diana
Mai, Nghia
Mancinelli, Rocco
McIntyre, Michael
Minelli, Giovanni
Neumann, Michael
Parra, Macarena
Piccini, Matthew
Rasay, R. Mike
Ricks, Robert
Santos, Orlando
Schooley, Aaron
Squires, David
Timucin, Linda
Yost, Bruce
Young, Anthony
TI The O/OREOS Mission: First Science Data from the Space Environment
Survivability of Living Organisms (SESLO) Payload
SO ASTROBIOLOGY
LA English
DT Article
DE Astrobiology; Bacillus subtilis; Germination; Low Earth orbit;
Microfluidics; NanosatelliteO/OREOS-Spores
ID IONIZING-RADIATION; DNA-REPAIR; RESISTANCE
AB We report the first telemetered spaceflight science results from the orbiting Space Environment Survivability of Living Organisms (SESLO) experiment, executed by one of the two 10 cm cube-format payloads aboard the 5.5 kg Organism/Organic Exposure to Orbital Stresses (O/OREOS) free-flying nanosatellite. The O/OREOS spacecraft was launched successfully to a 72 degrees inclination, 650km Earth orbit on 19 November 2010. This satellite provides access to the radiation environment of space in relatively weak regions of Earth's protective magnetosphere as it passes close to the north and south magnetic poles; the total dose rate is about 15 times that in the orbit of the International Space Station. The SESLO experiment measures the long-term survival, germination, and growth responses, including metabolic activity, of Bacillus subtilis spores exposed to the microgravity, ionizing radiation, and heavy-ion bombardment of its high-inclination orbit. Six microwells containing wild-type (168) and six more containing radiation-sensitive mutant (WN1087) strains of dried B. subtilis spores were rehydrated with nutrient medium after 14 days in space to allow the spores to germinate and grow. Similarly, the same distribution of organisms in a different set of microwells was rehydrated with nutrient medium after 97 days in space. The nutrient medium included the redox dye Alamar blue, which changes color in response to cellular metabolic activity. Three-color transmitted intensity measurements of all microwells were telemetered to Earth within days of each of the 48 h growth experiments. We report here on the evaluation and interpretation of these spaceflight data in comparison to delayed-synchronous laboratory ground control experiments.
C1 [Nicholson, Wayne L.] Univ Florida, Dept Microbiol & Cell Sci, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA.
[Ricco, Antonio J.; Agasid, Elwood; Beasley, Christopher; Diaz-Aguado, Millan; Friedericks, Charles; Ghassemieh, Shakib; Henschke, Michael; Hines, John W.; Luzzi, Ed; Ly, Diana; Mai, Nghia; McIntyre, Michael; Minelli, Giovanni; Parra, Macarena; Piccini, Matthew; Ricks, Robert; Santos, Orlando; Schooley, Aaron; Squires, David; Timucin, Linda; Yost, Bruce] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA.
[Kitts, Christopher; Mancinelli, Rocco] Bay Area Environm Res Inst, Sonoma, CA USA.
[Neumann, Michael; Rasay, R. Mike; Young, Anthony] Santa Clara Univ, Robot Syst Lab, Santa Clara, CA 95053 USA.
RP Nicholson, WL (reprint author), Univ Florida, Dept Microbiol & Cell Sci, Space Life Sci Lab, Bldg M6-1025,Room 201-B, Kennedy Space Ctr, FL 32899 USA.
EM WLN@ufl.edu
RI Ricco, Antonio/A-5273-2010; Mavoa, Suzanne/B-5372-2010;
OI Ricco, Antonio/0000-0002-2355-4984
FU NASA Planetary Protection Office [NNA06CB58G, NNX10AV22G]; NASA
Astrobiology
FX Thanks go to Patricia Fajardo-Cavazos and Ralf Moeller for valuable
technical support and discussions. This work was supported in part by
grants from the NASA Planetary Protection Office (NNA06CB58G and
NNX10AV22G) to W.L.N. The O/OREOS mission is the first nanosatellite for
the NASA Astrobiology Small-Payloads Program, which we acknowledge for
financial support of its development and this mission; we thank in
particular John Rummel, Cassie Conley, and Mary Voytek. Without the NASA
Ames Small Spacecraft Payloads and Technologies team comprised of
talented engineers, managers, students, and scientists, the mission
would not have been such a success. Specifically the team would like to
acknowledge Cindy Taylor, Emmett Quigley, Greg Defouw, Matthew Lera,
Mike Cohen, Karolyn Ronzano, Jeffrey Lin, Christina Mayberry, Roland
Burton, Lynn Hofland, and John Tucker. We are also very grateful for the
efforts of the highly effective student-and-staff operations team at
Santa Clara University, including Laura Bica and Ignacio Mas. We
acknowledge helpful discussions and guidance from David Landis (Draper
Laboratory) and Andrew Holmes-Siedle (REM Oxford, Ltd.), developers of
the SEVO spectrometer and the radFETs, respectively. Many others have
also contributed to the mission including USAF STP, Orbital Sciences,
and California Polytechnic University, San Luis Obispo.
NR 18
TC 19
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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 DEC
PY 2011
VL 11
IS 10
BP 951
EP 958
DI 10.1089/ast.2011.0714
PG 8
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 865YA
UT WOS:000298345600002
PM 22091486
ER
PT J
AU Schulze-Makuch, D
Mendez, A
Fairen, AG
von Paris, P
Turse, C
Boyer, G
Davila, AF
Antonio, MRD
Catling, D
Irwin, LN
AF Schulze-Makuch, Dirk
Mendez, Abel
Fairen, Alberto G.
von Paris, Philip
Turse, Carol
Boyer, Grayson
Davila, Alfonso F.
Antonio, Marina Resendes de Sousa
Catling, David
Irwin, Louis N.
TI A Two-Tiered Approach to Assessing the Habitability of Exoplanets
SO ASTROBIOLOGY
LA English
DT Article
DE Habitability; Exoplanets; Index; Earth similarity; Complexity; Life
ID EARTH-LIKE PLANETS; TERRESTRIAL PLANETS; EXTRASOLAR PLANET; ALIEN LIFE;
ATMOSPHERE; OCEAN; TITAN; EVOLUTION; SEARCH; ENERGY
AB In the next few years, the number of catalogued exoplanets will be counted in the thousands. This will vastly expand the number of potentially habitable worlds and lead to a systematic assessment of their astrobiological potential. Here, we suggest a two-tiered classification scheme of exoplanet habitability. The first tier consists of an Earth Similarity Index (ESI), which allows worlds to be screened with regard to their similarity to Earth, the only known inhabited planet at this time. The ESI is based on data available or potentially available for most exoplanets such as mass, radius, and temperature. For the second tier of the classification scheme we propose a Planetary Habitability Index (PHI) based on the presence of a stable substrate, available energy, appropriate chemistry, and the potential for holding a liquid solvent. The PHI has been designed to minimize the biased search for life as we know it and to take into account life that might exist under more exotic conditions. As such, the PHI requires more detailed knowledge than is available for any exoplanet at this time. However, future missions such as the Terrestrial Planet Finder will collect this information and advance the PHI. Both indices are formulated in a way that enables their values to be updated as technology and our knowledge about habitable planets, moons, and life advances. Applying the proposed metrics to bodies within our Solar System for comparison reveals two planets in the Gliese 581 system, GJ 581 c and d, with an ESI comparable to that of Mars and a PHI between that of Europa and Enceladus.
C1 [Schulze-Makuch, Dirk; Turse, Carol; Antonio, Marina Resendes de Sousa] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
[Mendez, Abel] Univ Puerto Rico, Planetary Habitabil Lab, Arecibo, PR USA.
[Fairen, Alberto G.; Davila, Alfonso F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Fairen, Alberto G.; Davila, Alfonso F.] SETI Inst, Moffett Field, CA USA.
[von Paris, Philip] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, Berlin, Germany.
[Boyer, Grayson] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ USA.
[Catling, David] Univ Washington, Astrobiol Program, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Irwin, Louis N.] Univ Texas El Paso, Dept Biol Sci, El Paso, TX 79968 USA.
RP Schulze-Makuch, D (reprint author), Washington State Univ, Sch Earth & Environm Sci, POB 642812, Pullman, WA 99164 USA.
EM dirksm@wsu.edu
RI Davila, Alfonso/A-2198-2013;
OI Davila, Alfonso/0000-0002-0977-9909; Catling, David/0000-0001-5646-120X;
Schulze-Makuch, Dirk/0000-0002-1923-9746
FU Humboldt Foundation; Helmholtz Gemeinschaft
FX Dirk Schulze-Makuch thanks the Humboldt Foundation for their support,
and Philip von Paris acknowledges support from the Helmholtz
Gemeinschaft through the research alliance "Planetary Evolution and
Life."
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U1 5
U2 34
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 DEC
PY 2011
VL 11
IS 10
BP 1041
EP 1052
DI 10.1089/ast.2010.0592
PG 12
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 865YA
UT WOS:000298345600008
PM 22017274
ER
PT J
AU Debes, JH
Hoard, DW
Wachter, S
Leisawitz, DT
Cohen, M
AF Debes, John H.
Hoard, D. W.
Wachter, Stefanie
Leisawitz, David T.
Cohen, Martin
TI THE WIRED SURVEY. II. INFRARED EXCESSES IN THE SDSS DR7 WHITE DWARF
CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; planetary systems; white dwarfs
ID DIGITAL SKY SURVEY; SPITZER IRAC OBSERVATIONS; MAIN-SEQUENCE BINARIES;
GASEOUS DEBRIS DISC; WIDE-FIELD CAMERA; 7TH DATA RELEASE; BROWN DWARF;
SUBSTELLAR COMPANION; PHOTOMETRIC SYSTEM; PLANETARY SYSTEMS
AB With the launch of the Wide-field Infrared Survey Explorer (WISE), a new era of detecting planetary debris and brown dwarfs (BDs) around white dwarfs (WDs) has begun with the WISE InfraRed Excesses around Degenerates (WIRED) Survey. The WIRED Survey is sensitive to substellar objects and dusty debris around WDs out to distances exceeding 100 pc, well beyond the completeness level of local WDs. In this paper, we present a cross-correlation of the preliminary Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) WD catalog between the WISE, Two-Micron All Sky Survey (2MASS), UKIRT Infrared Deep Sky Survey (UKIDSS), and SDSS DR7 photometric catalogs. From similar to 18,000 input targets, there are WISE detections comprising 344 "naked" WDs (detection of the WD photosphere only), 1020 candidate WD+M dwarf binaries, 42 candidate WD+BD systems, 52 candidate WD+dust disk systems, and 69 targets with indeterminate infrared excess. We classified all of the detected targets through spectral energy distribution model fitting of the merged optical, near-IR, and WISE photometry. Some of these detections could be the result of contaminating sources within the large (approximate to 6 '') WISE point-spread function; we make a preliminary estimate for the rates of contamination for our WD+BD and WD+disk candidates and provide notes for each target of interest. Each candidate presented here should be confirmed with higher angular resolution infrared imaging or infrared spectroscopy. We also present an overview of the observational characteristics of the detected WDs in the WISE photometric bands, including the relative frequencies of candidate WD+M, WD+BD, and WD+disk systems.
C1 [Debes, John H.; Leisawitz, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Debes, John H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Wachter, Stefanie] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Cohen, Martin] Monterey Inst Res Astron, Marina, CA 93933 USA.
FU NASA; National Science Foundation; Alfred P. Sloan Foundation; U.S.
Department of Energy; 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; 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: (a) 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); (b) the Two Micron All Sky Survey (2MASS), 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; (c) the UKIRT Infrared Deep Sky Survey
(UKIDSS); (d) the Sloan Digital Sky Survey (SDSS). 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; (e) the
SIMBAD database, operated at CDS, Strasbourg, France; and (f) the
NASA/IPAC Infrared Science Archive, which is operated by JPL, Caltech,
under a contract with NASA. 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 79
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U1 1
U2 4
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 DEC
PY 2011
VL 197
IS 2
AR 38
DI 10.1088/0067-0049/197/2/38
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300024
ER
PT J
AU Grogin, NA
Kocevski, DD
Faber, SM
Ferguson, HC
Koekemoer, AM
Riess, AG
Acquaviva, V
Alexander, DM
Almaini, O
Ashby, MLN
Barden, M
Bell, EF
Bournaud, F
Brown, TM
Caputi, KI
Casertano, S
Cassata, P
Castellano, M
Challis, P
Chary, RR
Cheung, E
Cirasuolo, M
Conselice, CJ
Cooray, AR
Croton, DJ
Daddi, E
Dahlen, T
Dave, R
de Mello, DF
Dekel, A
Dickinson, M
Dolch, T
Donley, JL
Dunlop, JS
Dutton, AA
Elbaz, D
Fazio, GG
Filippenko, AV
Finkelstein, SL
Fontana, A
Gardner, JP
Garnavich, PM
Gawiser, E
Giavalisco, M
Grazian, A
Guo, YC
Hathi, NP
Haussler, B
Hopkins, PF
Huang, JS
Huang, KH
Jha, SW
Kartaltepe, JS
Kirshner, RP
Koo, DC
Lai, K
Lee, KS
Li, WD
Lotz, JM
Lucas, RA
Madau, P
McCarthy, PJ
McGrath, EJ
McIntosh, DH
McLure, RJ
Mobasher, B
Moustakas, LA
Mozena, M
Nandra, K
Newman, JA
Niemi, SM
Noeske, KG
Papovich, CJ
Pentericci, L
Pope, A
Primack, JR
Rajan, A
Ravindranath, S
Reddy, NA
Renzini, A
Rix, HW
Robaina, AR
Rodney, SA
Rosario, DJ
Rosati, P
Salimbeni, S
Scarlata, C
Siana, B
Simard, L
Smidt, J
Somerville, RS
Spinrad, H
Straughn, AN
Strolger, LG
Telford, O
Teplitz, HI
Trump, JR
van der Wel, A
Villforth, C
Wechsler, RH
Weiner, BJ
Wiklind, T
Wild, V
Wilson, G
Wuyts, S
Yan, HJ
Yun, MS
AF Grogin, Norman A.
Kocevski, Dale D.
Faber, S. M.
Ferguson, Henry C.
Koekemoer, Anton M.
Riess, Adam G.
Acquaviva, Viviana
Alexander, David M.
Almaini, Omar
Ashby, Matthew L. N.
Barden, Marco
Bell, Eric F.
Bournaud, Frederic
Brown, Thomas M.
Caputi, Karina I.
Casertano, Stefano
Cassata, Paolo
Castellano, Marco
Challis, Peter
Chary, Ranga-Ram
Cheung, Edmond
Cirasuolo, Michele
Conselice, Christopher J.
Cooray, Asantha Roshan
Croton, Darren J.
Daddi, Emanuele
Dahlen, Tomas
Dave, Romeel
de Mello, Duilia F.
Dekel, Avishai
Dickinson, Mark
Dolch, Timothy
Donley, Jennifer L.
Dunlop, James S.
Dutton, Aaron A.
Elbaz, David
Fazio, Giovanni G.
Filippenko, Alexei V.
Finkelstein, Steven L.
Fontana, Adriano
Gardner, Jonathan P.
Garnavich, Peter M.
Gawiser, Eric
Giavalisco, Mauro
Grazian, Andrea
Guo, Yicheng
Hathi, Nimish P.
Haeussler, Boris
Hopkins, Philip F.
Huang, Jia-Sheng
Huang, Kuang-Han
Jha, Saurabh W.
Kartaltepe, Jeyhan S.
Kirshner, Robert P.
Koo, David C.
Lai, Kamson
Lee, Kyoung-Soo
Li, Weidong
Lotz, Jennifer M.
Lucas, Ray A.
Madau, Piero
McCarthy, Patrick J.
McGrath, Elizabeth J.
McIntosh, Daniel H.
McLure, Ross J.
Mobasher, Bahram
Moustakas, Leonidas A.
Mozena, Mark
Nandra, Kirpal
Newman, Jeffrey A.
Niemi, Sami-Matias
Noeske, Kai G.
Papovich, Casey J.
Pentericci, Laura
Pope, Alexandra
Primack, Joel R.
Rajan, Abhijith
Ravindranath, Swara
Reddy, Naveen A.
Renzini, Alvio
Rix, Hans-Walter
Robaina, Aday R.
Rodney, Steven A.
Rosario, David J.
Rosati, Piero
Salimbeni, Sara
Scarlata, Claudia
Siana, Brian
Simard, Luc
Smidt, Joseph
Somerville, Rachel S.
Spinrad, Hyron
Straughn, Amber N.
Strolger, Louis-Gregory
Telford, Olivia
Teplitz, Harry I.
Trump, Jonathan R.
van der Wel, Arjen
Villforth, Carolin
Wechsler, Risa H.
Weiner, Benjamin J.
Wiklind, Tommy
Wild, Vivienne
Wilson, Grant
Wuyts, Stijn
Yan, Hao-Jing
Yun, Min S.
TI CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY
SURVEY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; galaxies: high-redshift
ID HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI;
LYMAN-BREAK GALAXIES; SUPERMASSIVE BLACK-HOLES; EXTENDED GROTH-STRIP;
GOODS-SOUTH FIELD; SIMILAR-TO 7; REST-FRAME ULTRAVIOLET; EARLY RELEASE
SCIENCE
AB The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) is designed to document the first third of galactic evolution, over the approximate redshift (z) range 8-1.5. It will image >250,000 distant galaxies using three separate cameras on the Hubble Space Telescope, from the mid-ultraviolet to the near-infrared, and will find and measure Type Ia supernovae at z > 1.5 to test their accuracy as standardizable candles for cosmology. Five premier multi-wavelength sky regions are selected, each with extensive ancillary data. The use of five widely separated fields mitigates cosmic variance and yields statistically robust and complete samples of galaxies down to a stellar mass of 10(9)M(circle dot) to z approximate to 2, reaching the knee of the ultraviolet luminosity function of galaxies to z approximate to 8. The survey covers approximately 800 arcmin(2) and is divided into two parts. The CANDELS/Deep survey (5 sigma point-source limit H = 27.7 mag) covers similar to 125 arcmin(2) within Great Observatories Origins Deep Survey (GOODS)-N and GOODS-S. The CANDELS/Wide survey includes GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-deep Survey) and covers the full area to a 5 sigma point-source limit of H greater than or similar to 27.0 mag. Together with the Hubble Ultra Deep Fields, the strategy creates a three-tiered "wedding-cake" approach that has proven efficient for extragalactic surveys. Data from the survey are nonproprietary and are useful for a wide variety of science investigations. In this paper, we describe the basic motivations for the survey, the CANDELS team science goals and the resulting observational requirements, the field selection and geometry, and the observing design. The Hubble data processing and products are described in a companion paper.
C1 [Grogin, Norman A.; Ferguson, Henry C.; Koekemoer, Anton M.; Brown, Thomas M.; Casertano, Stefano; Dahlen, Tomas; Donley, Jennifer L.; Huang, Kuang-Han; Lotz, Jennifer M.; Lucas, Ray A.; Niemi, Sami-Matias; Noeske, Kai G.; Rajan, Abhijith; Villforth, Carolin] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kocevski, Dale D.; Faber, S. M.; Cheung, Edmond; Koo, David C.; Lai, Kamson; Madau, Piero; McGrath, Elizabeth J.; Mozena, Mark; Trump, Jonathan R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Lick Observ, UCO, Santa Cruz, CA 95064 USA.
[Riess, Adam G.; Dolch, Timothy; Huang, Kuang-Han; Rodney, Steven A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Acquaviva, Viviana; Gawiser, Eric; Jha, Saurabh W.; Somerville, Rachel S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ USA.
[Alexander, David M.] Univ Durham, Dept Phys, Durham, England.
[Almaini, Omar; Conselice, Christopher J.; Haeussler, Boris] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Ashby, Matthew L. N.; Fazio, Giovanni G.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barden, Marco] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Bournaud, Frederic; Daddi, Emanuele; Elbaz, David] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Caputi, Karina I.; Dunlop, James S.; McLure, Ross J.; Wild, Vivienne] Univ Edinburgh, Inst Astron, Edinburgh, Midlothian, Scotland.
[Cassata, Paolo; Giavalisco, Mauro; Guo, Yicheng; Pope, Alexandra; Salimbeni, Sara; Wilson, Grant; Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Castellano, Marco; Fontana, Adriano; Grazian, Andrea; Pentericci, Laura] Osserv Astron Roma, INAF, I-00136 Rome, Italy.
[Challis, Peter] Harvard Coll Observ, Cambridge, MA USA.
[Chary, Ranga-Ram] CALTECH, US Planck Data Ctr, Pasadena, CA 91125 USA.
[Cirasuolo, Michele] UK Astron Technol Ctr, Edinburgh, Midlothian, Scotland.
[Cooray, Asantha Roshan; Smidt, Joseph] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Croton, Darren J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Dave, Romeel; Weiner, Benjamin J.] Univ Arizona, Dept Astron, Tucson, AZ USA.
[de Mello, Duilia F.; Gardner, Jonathan P.; Straughn, Amber N.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
[de Mello, Duilia F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Dickinson, Mark; Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Dutton, Aaron A.] Univ Victoria, Dept Phys & Astron, Victoria, BC, Canada.
[Filippenko, Alexei V.; Hopkins, Philip F.; Li, Weidong; Spinrad, Hyron] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Finkelstein, Steven L.; Papovich, Casey J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX USA.
[Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Hathi, Nimish P.; McCarthy, Patrick J.] Carnegie Observ, Pasadena, CA USA.
[Huang, Jia-Sheng] Smithsonian Inst Astrophys Observ, Cambridge, MA USA.
[Lee, Kyoung-Soo] Yale Ctr Astron & Astrophys, New Haven, CT USA.
[McIntosh, Daniel H.] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA.
[Mobasher, Bahram; Reddy, Naveen A.; Siana, Brian] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Nandra, Kirpal; Rosario, David J.; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany.
[Newman, Jeffrey A.; Telford, Olivia] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Ravindranath, Swara] Interuniv Ctr Astron & Astrophys, Pune, Maharashtra, India.
[Renzini, Alvio] Osserv Astron Padova, Padua, Italy.
[Rix, Hans-Walter; van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Robaina, Aday R.] Univ Barcelona, Inst Ciencies Cosmos, Barcelona, Spain.
[Rosati, Piero] European So Observ, D-37075 Garching, Germany.
[Scarlata, Claudia] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN USA.
[Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Simard, Luc] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC, Canada.
[Strolger, Louis-Gregory] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Teplitz, Harry I.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Wechsler, Risa H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Wiklind, Tommy] ESO, ALMA, Santiago, Chile.
[Yan, Hao-Jing] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
RP Grogin, NA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Daddi, Emanuele/D-1649-2012; Conselice, Christopher/B-4348-2013;
Bournaud, Frederic/K-1263-2013; Hathi, Nimish/J-7092-2014;
OI fontana, adriano/0000-0003-3820-2823; Koekemoer,
Anton/0000-0002-6610-2048; Brown, Thomas/0000-0002-1793-9968; Bell,
Eric/0000-0002-5564-9873; Moustakas, Leonidas/0000-0003-3030-2360;
Alexander, David/0000-0002-5896-6313; Daddi,
Emanuele/0000-0002-3331-9590; Hathi, Nimish/0000-0001-6145-5090;
Castellano, Marco/0000-0001-9875-8263; Conselice,
Christopher/0000-0003-1949-7638; Cheung, Edmond/0000-0001-8546-1428
FU NASA through the Space Telescope Science Institute [GO-12060, GO-12099];
NASA [NAS5-26555]; ASI-INAF [I/009/10/0]
FX Support for HST Programs GO-12060 and GO-12099 was provided by NASA
through grants from the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS5-26555. A. Fontana acknowledges support
from agreement ASI-INAF I/009/10/0.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
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SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300021
ER
PT J
AU Hurley, K
Atteia, JL
Barraud, C
Pelangeon, A
Boer, M
Vanderspek, R
Ricker, G
Mazets, E
Golenetskii, S
Frederiks, DD
Pal'shin, VD
Aptekar, RL
Smith, DM
Wigger, C
Hajdas, W
Rau, A
von Kienlin, A
Mitrofanov, IG
Golovin, DV
Kozyrev, AS
Litvak, ML
Sanin, AB
Boynton, W
Fellows, C
Harshman, K
Barthelmy, S
Cline, T
Cummings, J
Gehrels, N
Krimm, HA
Yamaoka, K
Fukazawa, Y
Hanabata, Y
Ohno, M
Takahashi, T
Tashiro, M
Terada, Y
Murakami, T
Makishima, K
Guidorzi, C
Frontera, F
Montanari, CE
Rossi, F
Trombka, J
McClanahan, T
Starr, R
Goldsten, J
Gold, R
AF Hurley, K.
Atteia, J. -L.
Barraud, C.
Pelangeon, A.
Boer, M.
Vanderspek, R.
Ricker, G.
Mazets, E.
Golenetskii, S.
Frederiks, D. D.
Pal'shin, V. D.
Aptekar, R. L.
Smith, D. M.
Wigger, C.
Hajdas, W.
Rau, A.
von Kienlin, A.
Mitrofanov, I. G.
Golovin, D. V.
Kozyrev, A. S.
Litvak, M. L.
Sanin, A. B.
Boynton, W.
Fellows, C.
Harshman, K.
Barthelmy, S.
Cline, T.
Cummings, J.
Gehrels, N.
Krimm, H. A.
Yamaoka, K.
Fukazawa, Y.
Hanabata, Y.
Ohno, M.
Takahashi, T.
Tashiro, M.
Terada, Y.
Murakami, T.
Makishima, K.
Guidorzi, C.
Frontera, F.
Montanari, C. E.
Rossi, F.
Trombka, J.
McClanahan, T.
Starr, R.
Goldsten, J.
Gold, R.
TI THE INTERPLANETARY NETWORK SUPPLEMENT TO THE HETE-2 GAMMA-RAY BURST
CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma-ray burst: general; space vehicles: instruments
ID ARRIVAL-TIME LOCALIZATIONS; PIONEER-VENUS-ORBITER; ALL-SKY MONITOR;
ULYSSES SUPPLEMENT; BEPPOSAX; PERFORMANCE; MISSION; SPECTROMETER;
EXPLORER
AB Between 2000 November and 2006 May, one or more spacecraft of the interplanetary network (IPN) detected 226 cosmic gamma-ray bursts that were also detected by the French Gamma-Ray Telescope experiment on board the High Energy Transient Experiment 2 spacecraft. During this period, the IPN consisted of up to nine spacecraft, and using triangulation, the localizations of 157 bursts were obtained. We present the IPN localization data on these events.
C1 [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Atteia, J. -L.; Barraud, C.; Pelangeon, A.] Univ Toulouse, IRAP, CNRS, F-31400 Toulouse, France.
[Boer, M.] Observ Haute Provence, F-04870 St Michel lObservatoire, France.
[Vanderspek, R.; Ricker, G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Mazets, E.; Golenetskii, S.; Frederiks, D. D.; Pal'shin, V. D.; Aptekar, R. L.] Russian Acad Sci, AF Ioffe Physicotech Inst, St Petersburg 194021, Russia.
[Smith, D. M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Smith, D. M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Wigger, C.; Hajdas, W.] Paul Scherrer Inst, CH-5232 Villigen, Switzerland.
[Rau, A.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Mitrofanov, I. G.; Golovin, D. V.; Kozyrev, A. S.; Litvak, M. L.; Sanin, A. B.] Space Res Inst, Moscow 117997, Russia.
[Boynton, W.; Fellows, C.; Harshman, K.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Barthelmy, S.; Cline, T.; Cummings, J.; Gehrels, N.; Krimm, H. A.; Trombka, J.; McClanahan, T.; Starr, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yamaoka, K.] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2298558, Japan.
[Fukazawa, Y.; Hanabata, Y.; Ohno, M.] Hiroshima Univ, Dept Phys, Higashihiroshima, Hiroshima 7398526, Japan.
[Takahashi, T.] Inst Space & Astronaut Sci ISAS JAXA, Sagamihara, Kanagawa 2298510, Japan.
[Tashiro, M.; Terada, Y.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan.
[Murakami, T.] Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan.
[Makishima, K.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Guidorzi, C.; Frontera, F.; Montanari, C. E.; Rossi, F.] Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy.
[Goldsten, J.; Gold, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Wigger, C.] Kantonssch Baden, CH-5400 Baden, Switzerland.
[Cummings, J.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Makishima, K.] Inst Phys & Chem Res RIKEN, Makishima Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Frontera, F.] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy.
[Montanari, C. E.] Ist IS Calvi, Finale Emilia, MO, Italy.
RP Hurley, K (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM khurley@ssl.berkeley.edu
RI McClanahan, Timothy/C-8164-2012; Barthelmy, Scott/D-2943-2012; Gehrels,
Neil/D-2971-2012; Tashiro, Makoto/J-4562-2012; Terada,
Yukikatsu/A-5879-2013; Frederiks, Dmitry/C-7612-2014; Pal'shin,
Valentin/F-3973-2014; Aptekar, Raphail/B-3456-2015; Golenetskii,
Sergey/B-3818-2015;
OI Terada, Yukikatsu/0000-0002-2359-1857; Frederiks,
Dmitry/0000-0002-1153-6340
FU JPL [958056, 1268385]; MIT [SC-R-293291]; NASA [NAG5-11451, NNX07AH52G,
NAG5-13080, NAG5-12614, NNG04GM50G, NNG05GF72G, NAG5-9126, NNX06AI36G,
NAG5-9503, NNX07AR71G]; JPL (Odyssey) [1282043]; Federal Space Agency of
Russia; RFBR [09-02-00166a]; ASI-INAF [I/088/06/0]
FX Between 2000 and 2006, support for the interplanetary network came from
the following sources: JPL Contracts 958056 and 1268385 (Ulysses), MIT
Contract SC-R-293291 and NASA NAG5-11451 (HETE), NASA NNX07AH52G
(Konus), NASA NAG5-13080 (RHESSI), NASA NAG5-12614 and NNG04GM50G
(INTEGRAL), NASA NAG5-11451 and JPL Contract 1282043 (Odyssey), NASA
NNG05GF72G (Swift), NASA NAG5-9126 (BeppoSAX), NASA NNX06AI36G (Suzaku),
NASA NAG5-9503 (NEAR), and NASA NNX07AR71G (MESSENGER). In Russia, this
work was supported by the Federal Space Agency of Russia and RFBR Grant
09-02-00166a. C.G., F.F., and E.M. acknowledge financial support by
ASI-INAF contract I/088/06/0.
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PI BRISTOL
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.
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PG 13
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SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300020
ER
PT J
AU Johnson, JA
Clanton, C
Howard, AW
Bowler, BP
Henry, GW
Marcy, GW
Crepp, JR
Endl, M
Cochran, WD
MacQueen, PJ
Wright, JT
Isaacson, H
AF Johnson, John Asher
Clanton, Christian
Howard, Andrew W.
Bowler, Brendan P.
Henry, Gregory W.
Marcy, Geoffrey W.
Crepp, Justin R.
Endl, Michael
Cochran, William D.
MacQueen, Phillip J.
Wright, Jason T.
Isaacson, Howard
TI RETIRED A STARS AND THEIR COMPANIONS. VII. 18 NEW JOVIAN PLANETS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: spectroscopic; planetary systems; techniques: photometric;
techniques: radial velocities
ID HOBBY-EBERLY TELESCOPE; RADIAL-VELOCITY MEASUREMENTS; INTERMEDIATE-MASS
STARS; METAL-RICH STARS; HOST STARS; EXTRASOLAR PLANETS; N2K CONSORTIUM;
SEARCH PROGRAM; EVOLVED STARS; GIANT PLANETS
AB We report the detection of 18 Jovian planets discovered as part of our Doppler survey of subgiant stars at Keck Observatory, with follow-up Doppler and photometric observations made at McDonald and Fairborn Observatories, respectively. The host stars have masses 0.927 <= M(star)/M(circle dot) <= 1.95, radii 2.5 <= R(star)/R(circle dot) <= 8.7, and metallicities -0.46 <= [Fe/H] <= +0.30. The planets have minimum masses 0.9 M(Jup) <= M(P) sin i less than or similar to 13 M(Jup) and semimajor axes a >= 0.76 AU. These detections represent a 50% increase in the number of planets known to orbit stars more massive than 1.5M(circle dot) and provide valuable additional information about the properties of planets around stars more massive than the Sun.
C1 [Johnson, John Asher; Clanton, Christian; Crepp, Justin R.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Johnson, John Asher; Clanton, Christian] NASA, Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA.
[Howard, Andrew W.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Bowler, Brendan P.; Isaacson, Howard] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
[Endl, Michael; Cochran, William D.; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
RP Johnson, JA (reprint author), CALTECH, Dept Astrophys, MC 249-17, Pasadena, CA 91125 USA.
EM johnjohn@astro.caltech.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Wright, Jason/0000-0001-6160-5888
FU NSF [AST-0702821]; NASA Exoplanets Science Institute (NExScI); NASA
[NNX06AH52G]; Center for Exoplanets and Habitable Worlds; Pennsylvania
State University; Eberly College of Science; Pennsylvania Space Grant
Consortium; Tennessee State University; State of Tennessee through its
Centers of Excellence
FX We thank the many observers who contributed to the observations reported
here. We gratefully acknowledge the efforts and dedication of the Keck
Observatory staff, especially Grant Hill, Scott Dahm, and Hien Tran for
their support of HIRES and Greg Wirth for support of remote observing.
We are also grateful to the time assignment committees of NASA, NOAO,
Caltech, and the University of California for their generous allocations
of observing time. J.A.J. thanks the NSF Astronomy and Astrophysics
Postdoctoral Fellowship program for support in the years leading to the
completion of this work and acknowledges support from NSF grant
AST-0702821 and the NASA Exoplanets Science Institute (NExScI). G. W. M.
acknowledges NASA grant NNX06AH52G. J.T.W. was partially supported by
funding from the Center for Exoplanets and Habitable Worlds. The Center
for Exoplanets and Habitable Worlds is supported by the Pennsylvania
State University, the Eberly College of Science, and the Pennsylvania
Space Grant Consortium. G. W. H acknowledges support from NASA, NSF,
Tennessee State University, and the State of Tennessee through its
Centers of Excellence program. Finally, the authors wish to extend
special thanks to those of Hawaiian ancestry on whose sacred mountain of
Mauna Kea we are privileged to be guests. Without their generous
hospitality, the Keck observations presented herein would not have been
possible.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300012
ER
PT J
AU Kirkpatrick, JD
Cushing, MC
Gelino, CR
Griffith, RL
Skrutskie, MF
Marsh, KA
Wright, EL
Mainzer, A
Eisenhardt, PR
McLean, IS
Thompson, MA
Bauer, JM
Benford, DJ
Bridge, CR
Lake, SE
Petty, SM
Stanford, SA
Tsai, CW
Bailey, V
Beichman, CA
Bloom, JS
Bochanski, JJ
Burgasser, AJ
Capak, PL
Cruz, KL
Hinz, PM
Kartaltepe, JS
Knox, RP
Manohar, S
Masters, D
Morales-Calderon, M
Prato, LA
Rodigas, TJ
Salvato, M
Schurr, SD
Scoville, NZ
Simcoe, RA
Stapelfeldt, KR
Stern, D
Stock, ND
Vacca, WD
AF Kirkpatrick, J. Davy
Cushing, Michael C.
Gelino, Christopher R.
Griffith, Roger L.
Skrutskie, Michael F.
Marsh, Kenneth A.
Wright, Edward L.
Mainzer, A.
Eisenhardt, Peter R.
McLean, Ian S.
Thompson, Maggie A.
Bauer, James M.
Benford, Dominic J.
Bridge, Carrie R.
Lake, Sean E.
Petty, Sara M.
Stanford, S. A.
Tsai, Chao-Wei
Bailey, Vanessa
Beichman, Charles A.
Bloom, Joshua S.
Bochanski, John J.
Burgasser, Adam J.
Capak, Peter L.
Cruz, Kelle L.
Hinz, Philip M.
Kartaltepe, Jeyhan S.
Knox, Russell P.
Manohar, Swarnima
Masters, Daniel
Morales-Calderon, Maria
Prato, Lisa A.
Rodigas, Timothy J.
Salvato, Mara
Schurr, Steven D.
Scoville, Nicholas Z.
Simcoe, Robert A.
Stapelfeldt, Karl R.
Stern, Daniel
Stock, Nathan D.
Vacca, William D.
TI THE FIRST HUNDRED BROWN DWARFS DISCOVERED BY THE WIDE-FIELD INFRARED
SURVEY EXPLORER (WISE)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE brown dwarfs; infrared: stars; parallaxes; proper motions; solar
neighborhood; stars: luminosity function; mass function
ID DIGITAL SKY SURVEY; PROPER-MOTION SURVEY; LOW-MASS STARS; SURVEY
COMMISSIONING DATA; SPITZER-SPACE-TELESCOPE; BLUE L DWARF; ADAPTIVE
OPTICS SYSTEM; KECK-II-TELESCOPE; LARGE-AREA SURVEY; METHANE T-DWARFS
AB We present ground-based spectroscopic verification of 6 Y dwarfs (see also Cushing et al.), 89 T dwarfs, 8 L dwarfs, and 1 M dwarf identified by the Wide-field Infrared Survey Explorer (WISE). Eighty of these are cold brown dwarfs with spectral types >= T6, six of which have been announced earlier by Mainzer et al. and Burgasser et al. We present color-color and color-type diagrams showing the locus of M, L, T, and Y dwarfs in WISE color space. Near-infrared and, in a few cases, optical spectra are presented for these discoveries. Near-infrared classifications as late as early Y are presented and objects with peculiar spectra are discussed. Using these new discoveries, we are also able to extend the optical T dwarf classification scheme from T8 to T9. After deriving an absolute WISE 4.6 mu m (W2) magnitude versus spectral type relation, we estimate spectrophotometric distances to our discoveries. We also use available astrometric measurements to provide preliminary trigonometric parallaxes to four of our discoveries, which have types of L9 pec (red), T8, T9, and Y0; all of these lie within 10 pc of the Sun. The Y0 dwarf, WISE 1541-2250, is the closest at 2.8(-0.6)(+1.3) pc; if this 2.8 pc value persists after continued monitoring, WISE 1541-2250 will become the seventh closest stellar system to the Sun. Another 10 objects, with types between T6 and >Y0, have spectrophotometric distance estimates also placing them within 10 pc. The closest of these, the T6 dwarf WISE 1506+7027, is believed to fall at a distance of similar to 4.9 pc. WISE multi-epoch positions supplemented with positional info primarily from the Spitzer/Infrared Array Camera allow us to calculate proper motions and tangential velocities for roughly one-half of the new discoveries. This work represents the first step by WISE to complete a full-sky, volume-limited census of late-T and Y dwarfs. Using early results from this census, we present preliminary, lower limits to the space density of these objects and discuss constraints on both the functional form of the mass function and the low-mass limit of star formation.
C1 [Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Marsh, Kenneth A.; Tsai, Chao-Wei; Beichman, Charles A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Cushing, Michael C.; Mainzer, A.; Eisenhardt, Peter R.; Bauer, James M.; Stapelfeldt, Karl R.; Stern, Daniel] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Wright, Edward L.; McLean, Ian S.; Lake, Sean E.; Petty, Sara M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Thompson, Maggie A.] Potomac Sch, Mclean, VA 22101 USA.
[Benford, Dominic J.] NASA, Infrared Astrophys Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bridge, Carrie R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Bailey, Vanessa; Hinz, Philip M.; Knox, Russell P.; Rodigas, Timothy J.; Stock, Nathan D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bloom, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Bochanski, John J.; Simcoe, Robert A.] MIT, Cambridge, MA 02139 USA.
[Bochanski, John J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Burgasser, Adam J.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Capak, Peter L.; Morales-Calderon, Maria] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Cruz, Kelle L.] Hunter Coll, Dept Phys & Astron, New York, NY 10065 USA.
[Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Masters, Daniel] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Prato, Lisa A.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Salvato, Mara] Max Planck Inst Plasma Phys, D-85741 Garching, Germany.
[Schurr, Steven D.] CALTECH, Planck Sci Ctr, Pasadena, CA 91125 USA.
[Vacca, William D.] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kirkpatrick, JD (reprint author), CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA.
EM davy@ipac.caltech.edu
RI Benford, Dominic/D-4760-2012; Stapelfeldt, Karl/D-2721-2012;
Morales-Calderon, Maria/C-8384-2017;
OI Benford, Dominic/0000-0002-9884-4206; Morales-Calderon,
Maria/0000-0001-9526-9499; Bailey, Vanessa/0000-0002-5407-2806
FU National Aeronautics and Space Administration [NAS 5-26555, NNX10AI28G];
National Science Foundation; Alfred P. Sloan Foundation; U.S. Department
of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education
Funding Council for England; Space Telescope Science Institute under
U.S. Government [NAG W-2166]; NASA by JPL/Caltech [70062]; NASA through
the Space Telescope Science Institute [12330]; W. M. Keck Foundation;
Harvard University; University of Virginia; National Optical Astronomy
Observatory (NOAO) [2010B-0184]
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. We acknowledge fruitful discussions with Tim Conrow, Roc
Cutri, and Frank Masci, and acknowledge assistance with Magellan/FIRE
observations by Emily Bowsher. This publication also makes use of data
products from 2MASS, SDSS, and UKIDSS. 2MASS is a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the National
Aeronautics and Space Administration and the National Science
Foundation. SDSS is funded by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, the U.S.
Department of Energy, the National Aeronautics and Space Administration,
the Japanese Monbukagakusho, the Max Planck Society, and the Higher
Education Funding Council for England. UKIDSS uses the Wide Field Camera
at the United Kingdom Infrared Telescope atop Mauna Kea, Hawai'i. We are
grateful for the efforts of the instrument, calibration, and pipeline
teams that have made the UKIDSS data possible. We acknowledge use of the
DSS, 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. This research has made
use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated
by the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
Our research has benefited from the M, L, and T dwarf compendium housed
at DwarfArchives.org, whose server was funded by a NASA Small Research
Grant, administered by the American Astronomical Society. We are also
indebted to the SIMBAD database, operated at CDS, Strasbourg, France.
This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Support
for this work was provided by NASA through an award issued to program
70062 by JPL/Caltech. This work is also based in part on observations
made with the NASA/ESA Hubble Space Telescope, obtained at the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555. These observations are associated with program 12330. Support
for program 12330 was provided by NASA through a grant from the Space
Telescope Science Institute. Some of the spectroscopic data presented
herein were obtained at the W. M. Keck Observatory, which is operated as
a scientific partnership among the California Institute of Technology,
the University of California and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous
financial support of the W. M. Keck Foundation. In acknowledgement of
our observing time at Keck and the IRTF, we further wish to recognize
the very significant cultural role and reverence that the summit of
Mauna Kea has always had within the indigenous Hawai'ian community. We
are most fortunate to have the opportunity to conduct observations from
this mountain.; We acknowledge use of PAIRITEL, which is operated by the
Smithsonian Astrophysical Observtory (SAO) and was made possible by a
grant from the Harvard University Milton Fund, the camera loaned from
the University of Virginia, and the continued support of the SAO and UC
Berkeley. The PAIRITEL project is supported by NASA Grant NNX10AI28G. We
thank Dan Starr, Cullen Blake, Adam Morgan, Adam Miller, and Chris Klein
for their assistance. This paper also includes data gathered with the
6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
Portions of our Magellan telescope time were granted by the National
Optical Astronomy Observatory (NOAO; Proposal ID 2010B-0184), through
the Telescope System Instrumentation Program (TSIP). TSIP is funded by
NOAO, which is operated by the Association of Universities for Research
in Astronomy under cooperative agreement with the National Science
Foundation. We thank Alan Tokunaga for granting director's discretionary
time with IRTF/SpeX for some of the observations presented herein.
NR 199
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD DEC
PY 2011
VL 197
IS 2
AR 19
DI 10.1088/0067-0049/197/2/19
PG 55
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300005
ER
PT J
AU Koekemoer, AM
Faber, SM
Ferguson, HC
Grogin, NA
Kocevski, DD
Koo, DC
Lai, K
Lotz, JM
Lucas, RA
McGrath, EJ
Ogaz, S
Rajan, A
Riess, AG
Rodney, SA
Strolger, L
Casertano, S
Castellano, M
Dahlen, T
Dickinson, M
Dolch, T
Fontana, A
Giavalisco, M
Grazian, A
Guo, YC
Hathi, NP
Huang, KH
van der Wel, A
Yan, HJ
Acquaviva, V
Alexander, DM
Almaini, O
Ashby, MLN
Barden, M
Bell, EF
Bournaud, F
Brown, TM
Caputi, KI
Cassata, P
Challis, PJ
Chary, RR
Cheung, E
Cirasuolo, M
Conselice, CJ
Cooray, AR
Croton, DJ
Daddi, E
Dave, R
de Mello, DF
de Ravel, L
Dekel, A
Donley, JL
Dunlop, JS
Dutton, AA
Elbaz, D
Fazio, GG
Filippenko, AV
Finkelstein, SL
Frazer, C
Gardner, JP
Garnavich, PM
Gawiser, E
Gruetzbauch, R
Hartley, WG
Haussler, B
Herrington, J
Hopkins, PF
Huang, JS
Jha, SW
Johnson, A
Kartaltepe, JS
Khostovan, AA
Kirshner, RP
Lani, C
Lee, KS
Li, WD
Madau, P
McCarthy, PJ
McIntosh, DH
McLure, RJ
McPartland, C
Mobasher, B
Moreira, H
Mortlock, A
Moustakas, LA
Mozena, M
Nandra, K
Newman, JA
Nielsen, JL
Niemi, S
Noeske, KG
Papovich, CJ
Pentericci, L
Pope, A
Primack, JR
Ravindranath, S
Reddy, NA
Renzini, A
Rix, HW
Robaina, AR
Rosario, DJ
Rosati, P
Salimbeni, S
Scarlata, C
Siana, B
Simard, L
Smidt, J
Snyder, D
Somerville, RS
Spinrad, H
Straughn, AN
Telford, O
Teplitz, HI
Trump, JR
Vargas, C
Villforth, C
Wagner, CR
Wandro, P
Wechsler, RH
Weiner, BJ
Wiklind, T
Wild, V
Wilson, G
Wuyts, S
Yun, MS
AF Koekemoer, Anton M.
Faber, S. M.
Ferguson, Henry C.
Grogin, Norman A.
Kocevski, Dale D.
Koo, David C.
Lai, Kamson
Lotz, Jennifer M.
Lucas, Ray A.
McGrath, Elizabeth J.
Ogaz, Sara
Rajan, Abhijith
Riess, Adam G.
Rodney, Steve A.
Strolger, Louis
Casertano, Stefano
Castellano, Marco
Dahlen, Tomas
Dickinson, Mark
Dolch, Timothy
Fontana, Adriano
Giavalisco, Mauro
Grazian, Andrea
Guo, Yicheng
Hathi, Nimish P.
Huang, Kuang-Han
van der Wel, Arjen
Yan, Hao-Jing
Acquaviva, Viviana
Alexander, David M.
Almaini, Omar
Ashby, Matthew L. N.
Barden, Marco
Bell, Eric F.
Bournaud, Frederic
Brown, Thomas M.
Caputi, Karina I.
Cassata, Paolo
Challis, Peter J.
Chary, Ranga-Ram
Cheung, Edmond
Cirasuolo, Michele
Conselice, Christopher J.
Cooray, Asantha Roshan
Croton, Darren J.
Daddi, Emanuele
Dave, Romeel
de Mello, Duilia F.
de Ravel, Loic
Dekel, Avishai
Donley, Jennifer L.
Dunlop, James S.
Dutton, Aaron A.
Elbaz, David
Fazio, Giovanni G.
Filippenko, Alexei V.
Finkelstein, Steven L.
Frazer, Chris
Gardner, Jonathan P.
Garnavich, Peter M.
Gawiser, Eric
Gruetzbauch, Ruth
Hartley, Will G.
Haeussler, Boris
Herrington, Jessica
Hopkins, Philip F.
Huang, Jia-Sheng
Jha, Saurabh W.
Johnson, Andrew
Kartaltepe, Jeyhan S.
Khostovan, Ali A.
Kirshner, Robert P.
Lani, Caterina
Lee, Kyoung-Soo
Li, Weidong
Madau, Piero
McCarthy, Patrick J.
McIntosh, Daniel H.
McLure, Ross J.
McPartland, Conor
Mobasher, Bahram
Moreira, Heidi
Mortlock, Alice
Moustakas, Leonidas A.
Mozena, Mark
Nandra, Kirpal
Newman, Jeffrey A.
Nielsen, Jennifer L.
Niemi, Sami
Noeske, Kai G.
Papovich, Casey J.
Pentericci, Laura
Pope, Alexandra
Primack, Joel R.
Ravindranath, Swara
Reddy, Naveen A.
Renzini, Alvio
Rix, Hans-Walter
Robaina, Aday R.
Rosario, David J.
Rosati, Piero
Salimbeni, Sara
Scarlata, Claudia
Siana, Brian
Simard, Luc
Smidt, Joseph
Snyder, Diana
Somerville, Rachel S.
Spinrad, Hyron
Straughn, Amber N.
Telford, Olivia
Teplitz, Harry I.
Trump, Jonathan R.
Vargas, Carlos
Villforth, Carolin
Wagner, Cory R.
Wandro, Pat
Wechsler, Risa H.
Weiner, Benjamin J.
Wiklind, Tommy
Wild, Vivienne
Wilson, Grant
Wuyts, Stijn
Yun, Min S.
TI CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY
SURVEY-THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS,
AND MOSAICS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; galaxies: high-redshift
ID STAR-FORMING GALAXIES; INTEGRAL FIELD SPECTROSCOPY; PROBE WMAP
OBSERVATIONS; UV LUMINOSITY FUNCTIONS; EXTENDED GROTH STRIP; EARLY DATA
RELEASE; HIGH-REDSHIFT; MASSIVE GALAXIES; IA SUPERNOVAE; SKY SURVEY
AB This paper describes the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). This survey is designed to document the evolution of galaxies and black holes at z approximate to 1.5-8, and to study Type Ia supernovae at z > 1.5. Five premier multi-wavelength sky regions are selected, each with extensive multi-wavelength observations. The primary CANDELS data consist of imaging obtained in the Wide Field Camera 3 infrared channel (WFC3/IR) and the WFC3 ultraviolet/optical channel, along with the Advanced Camera for Surveys (ACS). The CANDELS/Deep survey covers similar to 125 arcmin(2) within GOODS-N and GOODS-S, while the remainder consists of the CANDELS/Wide survey, achieving a total of similar to 800 arcmin(2) across GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-Deep Survey). We summarize the observational aspects of the survey as motivated by the scientific goals and present a detailed description of the data reduction procedures and products from the survey. Our data reduction methods utilize the most up-to-date calibration files and image combination procedures. We have paid special attention to correcting a range of instrumental effects, including charge transfer efficiency degradation for ACS, removal of electronic bias-striping present in ACS data after Servicing Mission 4, and persistence effects and other artifacts in WFC3/IR. For each field, we release mosaics for individual epochs and eventual mosaics containing data from all epochs combined, to facilitate photometric variability studies and the deepest possible photometry. A more detailed overview of the science goals and observational design of the survey are presented in a companion paper.
C1 [Koekemoer, Anton M.; Ferguson, Henry C.; Grogin, Norman A.; Lotz, Jennifer M.; Lucas, Ray A.; Ogaz, Sara; Rajan, Abhijith; Casertano, Stefano; Dahlen, Tomas; Huang, Kuang-Han; Brown, Thomas M.; Donley, Jennifer L.; Niemi, Sami; Noeske, Kai G.; Somerville, Rachel S.; Villforth, Carolin; Wiklind, Tommy] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Faber, S. M.; Kocevski, Dale D.; Koo, David C.; Lai, Kamson; McGrath, Elizabeth J.; Cheung, Edmond; Johnson, Andrew; Madau, Piero; McPartland, Conor; Mozena, Mark; Primack, Joel R.; Rosario, David J.; Snyder, Diana; Trump, Jonathan R.; Wandro, Pat] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Riess, Adam G.; Rodney, Steve A.; Dolch, Timothy; Huang, Kuang-Han; Kartaltepe, Jeyhan S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Strolger, Louis] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Castellano, Marco; Fontana, Adriano; Grazian, Andrea; Pentericci, Laura] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Dickinson, Mark; Pope, Alexandra; Reddy, Naveen A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Giavalisco, Mauro; Guo, Yicheng; Cassata, Paolo; Salimbeni, Sara; Wilson, Grant; Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Hathi, Nimish P.; McCarthy, Patrick J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[van der Wel, Arjen; Rix, Hans-Walter; Rosati, Piero] European So Observ, D-85748 Garching, Germany.
[Yan, Hao-Jing] Ohio State Univ, Res Fdn, Columbus, OH 43210 USA.
[Acquaviva, Viviana; Gawiser, Eric; Jha, Saurabh W.; Moreira, Heidi; Vargas, Carlos] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Almaini, Omar; Conselice, Christopher J.; Gruetzbauch, Ruth; Hartley, Will G.; Haeussler, Boris; Lani, Caterina; Mortlock, Alice] Univ Nottingham, Nottingham NG7 2RD, England.
[Ashby, Matthew L. N.; Fazio, Giovanni G.; Kirshner, Robert P.; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Barden, Marco] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Bell, Eric F.; Herrington, Jessica] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Bournaud, Frederic; Daddi, Emanuele] CEA, F-91191 Gif Sur Yvette, France.
[Bournaud, Frederic; Daddi, Emanuele] Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Caputi, Karina I.; Cirasuolo, Michele] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Challis, Peter J.] Harvard Coll Observ, Cambridge, MA USA.
[Cooray, Asantha Roshan; Frazer, Chris; Khostovan, Ali A.; Smidt, Joseph] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Croton, Darren J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Dave, Romeel; Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[de Mello, Duilia F.; Gardner, Jonathan P.; Straughn, Amber N.] NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Greenbelt, MD 20771 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Dutton, Aaron A.] Univ Victoria, Victoria, BC, Canada.
[Elbaz, David] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Filippenko, Alexei V.; Hopkins, Philip F.; Li, Weidong; Spinrad, Hyron] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Finkelstein, Steven L.; Papovich, Casey J.] Texas A&M Res Fdn, College Stn, TX 77843 USA.
[Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Huang, Jia-Sheng] Smithsonian Inst Astrophys Observ, Cambridge, MA USA.
[Lee, Kyoung-Soo] Yale Ctr Astron & Astrophys, New Haven, CT USA.
[McIntosh, Daniel H.; Nielsen, Jennifer L.; Wagner, Cory R.] Univ Missouri Kansas City, Dept Phys, Kansas City, MO 64110 USA.
[Mobasher, Bahram] UC Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nandra, Kirpal] Univ London Imperial Coll Sci Technol & Med, London, England.
[Newman, Jeffrey A.; Telford, Olivia] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Newman, Jeffrey A.] PITT PAC, Pittsburgh, PA USA.
[Ravindranath, Swara] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Renzini, Alvio] Osserv Astron Padova, Padua, Italy.
[Robaina, Aday R.] IEEC, Inst Ciencies Cosmos, ICC UB, Barcelona 08028, Spain.
[Wechsler, Risa H.] Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Wechsler, Risa H.] SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
RP Koekemoer, AM (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Daddi, Emanuele/D-1649-2012; Conselice, Christopher/B-4348-2013;
Bournaud, Frederic/K-1263-2013; Hathi, Nimish/J-7092-2014;
OI Koekemoer, Anton/0000-0002-6610-2048; Brown, Thomas/0000-0002-1793-9968;
Bell, Eric/0000-0002-5564-9873; Daddi, Emanuele/0000-0002-3331-9590;
Hathi, Nimish/0000-0001-6145-5090; Conselice,
Christopher/0000-0003-1949-7638; Cheung, Edmond/0000-0001-8546-1428;
Moustakas, Leonidas/0000-0003-3030-2360; fontana,
adriano/0000-0003-3820-2823
FU NASA through the Space Telescope Science Institute [GO-12060, GO-12099];
NASA [NAS5-26555]
FX We thank the referee for very helpful and valuable comments on this
manuscript. We also thank our Program Coordinators, Tricia Royle and
Beth Perriello, along with the rest of the Hubble planning team, for
their efforts to schedule this challenging program. The WFC3 team has
made substantial contributions to the program by calibrating and
characterizing the instrument and have provided much useful advice.
Rychard Bouwens provided helpful input on the observing strategy for the
CANDELS/Deep survey. John Mackenty suggested using 2 x 2 on-chip binning
for the UV observations, which will significantly improve the
signal-to-noise ratio of those observations. The CANDELS observations
would not have been possible without the contributions of hundreds of
other individuals to the Hubble missions and the development and
installation of new instruments. Support for HST Programs GO-12060 and
GO-12099 (the SN component) is 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
NAS5-26555.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD DEC
PY 2011
VL 197
IS 2
AR 36
DI 10.1088/0067-0049/197/2/36
PG 36
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300022
ER
PT J
AU Schwarz, GJ
Ness, JU
Osborne, JP
Page, KL
Evans, PA
Beardmore, AP
Walter, FM
Helton, LA
Woodward, CE
Bode, M
Starrfield, S
Drake, JJ
AF Schwarz, Greg J.
Ness, Jan-Uwe
Osborne, J. P.
Page, K. L.
Evans, P. A.
Beardmore, A. P.
Walter, Frederick M.
Helton, L. Andrew
Woodward, Charles E.
Bode, Mike
Starrfield, Sumner
Drake, Jeremy J.
TI SWIFT X-RAY OBSERVATIONS OF CLASSICAL NOVAE. II. THE SUPER SOFT SOURCE
SAMPLE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE novae, cataclysmic variables; ultraviolet: stars; X-rays: stars
ID INTERMEDIATE POLAR CANDIDATE; EXPANDING NEBULAR REMNANT; XMM-NEWTON
OBSERVATIONS; HIGH-SPEED PHOTOMETRY; V1974 CYGNI 1992; MIRA V407 CYG;
RS-OPHIUCHI; SPECTRAL EVOLUTION; RECURRENT NOVAE; 2006 OUTBURST
AB The Swift gamma-ray burst satellite is an excellent facility for studying novae. Its rapid response time and sensitive X-ray detector provides an unparalleled opportunity to investigate the previously poorly sampled evolution of novae in the X-ray regime. This paper presents Swift observations of 52 Galactic/Magellanic Cloud novae. We included the X-Ray Telescope (0.3-10 keV) instrument count rates and the UltraViolet and Optical Telescope (1700-8000 angstrom) filter photometry. Also included in the analysis are the publicly available pointed observations of 10 additional novae the X-ray archives. This is the largest X-ray sample of Galactic/Magellanic Cloud novae yet assembled and consists of 26 novae with Super Soft X-ray emission, 19 from Swift observations. The data set shows that the faster novae have an early hard X-ray phase that is usually missing in slower novae. The Super Soft X-ray phase occurs earlier and does not last as long in fast novae compared to slower novae. All the Swift novae with sufficient observations show that novae are highly variable with rapid variability and different periodicities. In the majority of cases, nuclear burning ceases less than three years after the outburst begins. Previous relationships, such as the nuclear burning duration versus t(2) or the expansion velocity of the eject and nuclear burning duration versus the orbital period, are shown to be poorly correlated with the full sample indicating that additional factors beyond the white dwarf mass and binary separation play important roles in the evolution of a nova outburst. Finally, we confirm two optical phenomena that are correlated with strong, soft X-ray emission which can be used to further increase the efficiency of X-ray campaigns.
C1 [Schwarz, Greg J.] Amer Astron Soc, Washington, DC 20009 USA.
[Ness, Jan-Uwe] ESAC, XMM Newton Sci Operat Ctr, Madrid 28691, Spain.
[Osborne, J. P.; Page, K. L.; Evans, P. A.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Walter, Frederick M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Helton, L. Andrew] NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Woodward, Charles E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Bode, Mike] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Starrfield, Sumner] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Drake, Jeremy J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Schwarz, GJ (reprint author), Amer Astron Soc, 2000 Florida Ave NW,Suite 400, Washington, DC 20009 USA.
EM Greg.Schwarz@aas.org
OI Schwarz, Gregory/0000-0002-0786-7307
FU NASA [NNH08ZDA001N1, NAS8-39073]; STFC; NSF
FX This research has made use of data obtained from NASA's Swift satellite.
We thank Neil Gehrels and the Swift team for generous allotments of ToO
and fill in time. Funding support from NASA NNH08ZDA001N1. Stony Brook
University's initial participation in the SMARTS consortium was made
possible by generous contributions from the Dean of Arts and Sciences,
the Provost, and the Vice President for Research of Stony Brook
University. We acknowledge with thanks the variable star observations
from the AAVSO International Database contributed by observers worldwide
and used in this research. J.P.O., K. P., P. E. and A. B. acknowledge
the support of the STFC. S. S. acknowledges partial support from NASA
and NSF grants to ASU. J.J.D. was supported by NASA contract NAS8-39073
to the Chandra X-ray Center.
NR 315
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD DEC
PY 2011
VL 197
IS 2
AR 31
DI 10.1088/0067-0049/197/2/31
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300017
ER
PT J
AU Wang, TJ
Thomas, RJ
Brosius, JW
Young, PR
Rabin, DM
Davila, JM
Del Zanna, G
AF Wang, Tongjiang
Thomas, Roger J.
Brosius, Jeffrey W.
Young, Peter R.
Rabin, Douglas M.
Davila, Joseph M.
Del Zanna, Giulio
TI UNDERFLIGHT CALIBRATION OF SOHO/CDS AND HINODE/EIS WITH EUNIS-07
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE instrumentation: spectrographs; Sun: activity; Sun: corona; Sun: UV
radiation
ID SOLAR ACTIVE-REGION; ULTRAVIOLET IMAGING SPECTROMETER; CORONAL
DIAGNOSTIC SPECTROMETER; EXTREME-ULTRAVIOLET; EMISSION-LINES; QUIET-SUN;
TRANSITION REGION; ATOMIC DATABASE; RADIOMETRIC CALIBRATION; IRRADIANCE
SPECTRUM
AB Flights of Goddard Space Flight Center's Extreme Ultraviolet Normal Incidence Spectrograph (EUNIS) sounding rocket in 2006 and 2007 provided updated radiometric calibrations for Solar and Heliospheric Observatory/Coronal Diagnostic Spectrometer (SOHO/CDS) and Hinode/Extreme Ultraviolet Imaging Spectrometer (Hinode/EIS). EUNIS carried two independent imaging spectrographs covering wavebands of 300-370 angstrom in first order and 170-205 angstrom in second order. After each flight, end-to-end radiometric calibrations of the rocket payload were carried out in the same facility used for pre-launch calibrations of CDS and EIS. During the 2007 flight, EUNIS, SOHO/CDS, and Hinode/EIS observed the same solar locations, allowing the EUNIS calibrations to be directly applied to both CDS and EIS. The measured CDS NIS 1 line intensities calibrated with the standard (version 4) responsivities with the standard long-term corrections are found to be too low by a factor of 1.5 due to the decrease in responsivity. The EIS calibration update is performed in two ways. One uses the direct calibration transfer of the calibrated EUNIS-07 short wavelength (SW) channel. The other uses the insensitive line pairs, in which one member was observed by the EUNIS-07 long wavelength (LW) channel and the other by EIS in either the LW or SW waveband. Measurements from both methods are in good agreement, and confirm (within the measurement uncertainties) the EIS responsivity measured directly before the instrument's launch. The measurements also suggest that the EIS responsivity decreased by a factor of about 1.2 after the first year of operation (although the size of the measurement uncertainties is comparable to this decrease). The shape of the EIS SW response curve obtained by EUNIS-07 is consistent with the one measured in laboratory prior to launch. The absolute value of the quiet-Sun He II 304 angstrom intensity measured by EUNIS-07 is consistent with the radiance measured by CDS NIS in quiet regions near the disk center and the solar minimum irradiance recently obtained by CDS NIS and the Solar Dynamics Observatory/Extreme Ultraviolet Variability Experiment.
C1 [Wang, Tongjiang; Brosius, Jeffrey W.] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA.
[Wang, Tongjiang; Thomas, Roger J.; Brosius, Jeffrey W.; Rabin, Douglas M.; Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Young, Peter R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Del Zanna, Giulio] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England.
RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, IACS, 620 Michigan Ave NE, Washington, DC 20064 USA.
EM tongjiang.wang@nasa.gov
FU NASA Heliophysics Division; NASA [NNX10AN10G, NNX08AE44G]; Naval
Research Laboratory; STFC (UK); Rutherford-Appleton Laboratory in
England; Physikalisch-Technische Bundesanstalt in Germany
FX The EUNIS program is supported by the NASA Heliophysics Division through
its Low Cost Access to Space Program in Solar and Heliospheric Physics.
T. W. is grateful to Drs. William T. Thompson, John Mariska, and
Vincenzo Andretta for their valuable comments. The work of T. W. was
supported by NASA grants NNX10AN10G and NNX08AE44G. The work of P.R.Y.
was performed under contract with the Naval Research Laboratory and was
funded by NASA. G.D.Z. acknowledges support from STFC (UK) via the
Advanced Fellowship programme. Radiometric calibration of the EUNIS-06
instrument was made possible by financial contributions and technical
support from both the Rutherford-Appleton Laboratory in England and the
Physikalisch-Technische Bundesanstalt in Germany, for which we are very
grateful. CHIANTI is a collaborative project involving the Universities
of Cambridge (UK), George Mason and Michigan (USA).
NR 52
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Z9 19
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD DEC
PY 2011
VL 197
IS 2
AR 32
DI 10.1088/0067-0049/197/2/32
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300018
ER
PT J
AU Wong, T
Hughes, A
Ott, J
Muller, E
Pineda, JL
Bernard, JP
Chu, YH
Fukui, Y
Gruendl, RA
Henkel, C
Kawamura, A
Klein, U
Looney, LW
Maddison, S
Mizuno, Y
Paradis, D
Seale, J
Welty, DE
AF Wong, Tony
Hughes, Annie
Ott, Juergen
Muller, Erik
Pineda, Jorge L.
Bernard, Jean-Philippe
Chu, You-Hua
Fukui, Yasuo
Gruendl, Robert A.
Henkel, Christian
Kawamura, Akiko
Klein, Ulrich
Looney, Leslie W.
Maddison, Sarah
Mizuno, Yoji
Paradis, Deborah
Seale, Jonathan
Welty, Daniel E.
TI THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD
POPULATION OF THE LARGE MAGELLANIC CLOUD
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: ISM; ISM: molecules; Magellanic Clouds; stars: formation
ID YOUNG STELLAR OBJECTS; SEST KEY PROGRAM; DENSITY
PROBABILITY-DISTRIBUTION; STAR-FORMATION; COLUMN DENSITY; CO SURVEY;
INTERSTELLAR-MEDIUM; DUST PROPERTIES; SPITZER SURVEY; LOCAL GROUP
AB We present the properties of an extensive sample of molecular clouds in the Large Magellanic Cloud (LMC) mapped at 11 pc resolution in the CO(1-0) line. Targets were chosen based on a limiting CO flux and peak brightness as measured by the NANTEN survey. The observations were conducted with the ATNF Mopra Telescope as part of the Magellanic Mopra Assessment. We identify clouds as regions of connected CO emission and find that the distributions of cloud sizes, fluxes, and masses are sensitive to the choice of decomposition parameters. In all cases, however, the luminosity function of CO clouds is steeper than dN/dL proportional to L(-2), suggesting that a substantial fraction of mass is in low-mass clouds. A correlation between size and linewidth, while apparent for the largest emission structures, breaks down when those structures are decomposed into smaller structures. We argue that the correlation between virial mass and CO luminosity is the result of comparing two covariant quantities, with the correlation appearing tighter on larger scales where a size-linewidth relation holds. The virial parameter (the ratio of a cloud's kinetic to self-gravitational energy) shows a wide range of values and exhibits no clear trends with the CO luminosity or the likelihood of hosting young stellar object (YSO) candidates, casting further doubt on the assumption of virialization for molecular clouds in the LMC. Higher CO luminosity increases the likelihood of a cloud harboring a YSO candidate, and more luminous YSOs are more likely to be coincident with detectable CO emission, confirming the close link between giant molecular clouds and massive star formation.
C1 [Wong, Tony; Chu, You-Hua; Gruendl, Robert A.; Looney, Leslie W.; Seale, Jonathan; Welty, Daniel E.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Hughes, Annie; Maddison, Sarah] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Hughes, Annie] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Hughes, Annie] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Ott, Juergen] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Muller, Erik; Fukui, Yasuo; Kawamura, Akiko; Mizuno, Yoji] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Muller, Erik; Kawamura, Akiko] Natl Inst Nat Sci, Natl Astron Observ Japan, ALMA J Project Off, Mitaka, Tokyo 1818588, Japan.
[Pineda, Jorge L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bernard, Jean-Philippe; Paradis, Deborah] IRAP, CNRS, F-31028 Toulouse 4, France.
[Bernard, Jean-Philippe; Paradis, Deborah] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Henkel, Christian] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Henkel, Christian] King Abdulaziz Univ, Fac Sci, Dept Astron, Jeddah, Saudi Arabia.
[Klein, Ulrich] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Seale, Jonathan] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Wong, T (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
EM wongt@astro.illinois.edu
RI Faculty of, Sciences, KAU/E-7305-2017
FU NSF [08-07323]; University of Illinois; NASA [10-ADAP10-0137]; Japan
Society for the Promotion of Science (KAKENHI) [22540250]
FX We are deeply indebted to the ATNF for the generous allocation of time
for this project and for assistance with planning and executing the
project over its duration of several years. Particular thanks go to
Michael Kesteven and Mark Calabretta for making the OTF mode at Mopra
possible, and to Balthasar Indermuehle for assistance with Mopra. T. W.
thanks Ned Ladd for assistance with developing the OTF mode. Lister
Staveley-Smith and Sungeun Kim furnished the Hi map of the LMC that
proved valuable for planning the observations. Erik Rosolowsky, Adam
Leroy, and Alberto Bolatto provided useful advice and suggestions on the
identification of clouds. We also benefited from stimulating discussions
with Remy Indebetouw and Rosie Chen. We thank the anonymous referee for
a number of helpful suggestions. Research by T. W. was supported by NSF
grant 08-07323, the University of Illinois, and NASA grant
10-ADAP10-0137. This research has been carried out in part at the Jet
Propulsion Laboratory, California Institute of Technology. A. K.
acknowledges support from the Japan Society for the Promotion of Science
(KAKENHI No. 22540250).
NR 64
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U1 0
U2 6
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 DEC
PY 2011
VL 197
IS 2
AR 16
DI 10.1088/0067-0049/197/2/16
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300002
ER
PT J
AU Parrish, DD
Singh, HB
Molina, L
Madronich, S
AF Parrish, David D.
Singh, Hanwant B.
Molina, Luisa
Madronich, Sasha
TI Air quality progress in North American megacities: A review
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Review
DE Air quality; Megacities; Ozone; Particulate matter; Pollution
ID VOLATILE ORGANIC-COMPOUNDS; AEROSOL MASS-SPECTROMETRY; CITY
METROPOLITAN-AREA; WRF-CHEM MODEL; MEXICO-CITY; CLIMATE-CHANGE;
UNITED-STATES; SOURCE APPORTIONMENT; INTEX-B; MCMA-2006/MILAGRO CAMPAIGN
AB Air quality progress in the North American megacities of Los Angeles, New York, and Mexico City is reviewed, compared, and contrasted. Enormous progress made in North America over the last 5 decades provides a template for other megacities of the world, especially in developing countries, attempting to achieve rapid economic growth without compromising air quality. While the progress to date has been impressive, many challenges remain including the need to improve air quality while simultaneously mitigating climate change. The impact of pollutant emissions from megacities is felt long distances away from the local sources but no policy mechanisms currently exist to mitigate air quality impacts resulting from such pollution transport. Published by Elsevier Ltd.
C1 [Parrish, David D.] NOAA, ESRL Chem Sci Div, Boulder, CO USA.
[Singh, Hanwant B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Molina, Luisa] Molina Ctr Energy & Environm, San Diego, CA USA.
[Madronich, Sasha] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Parrish, DD (reprint author), NOAA, ESRL Chem Sci Div, 325 Broadway R CSD7, Boulder, CO USA.
EM David.D.Parrish@noaa.gov
RI Parrish, David/E-8957-2010; Madronich, Sasha/D-3284-2015; Manager, CSD
Publications/B-2789-2015
OI Parrish, David/0000-0001-6312-2724; Madronich,
Sasha/0000-0003-0983-1313;
FU NASA; NOAA; National Center for Atmospheric Research; National Science
Foundation; MCE2
FX Research supported by NASA Tropospheric Chemistry Program, NOAA Health
of the Atmosphere Program, National Center for Atmospheric Research,
which is sponsored by the National Science Foundation and MCE2. The
authors thank Professors Arthur M. Winer of UCLA and Benjamin de Foy of
Saint Louis University for helpful discussion.
NR 93
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U2 110
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 DEC
PY 2011
VL 45
IS 39
BP 7015
EP 7025
DI 10.1016/j.atmosenv.2011.09.039
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 862UU
UT WOS:000298120400001
ER
PT J
AU Zoogman, P
Jacob, DJ
Chance, K
Zhang, L
Le Sager, P
Fiore, AM
Eldering, A
Liu, X
Natraj, V
Kulawik, SS
AF Zoogman, Peter
Jacob, Daniel J.
Chance, Kelly
Zhang, Lin
Le Sager, Philippe
Fiore, Arlene M.
Eldering, Annmarie
Liu, Xiong
Natraj, Vijay
Kulawik, Susan S.
TI Ozone air quality measurement requirements for a geostationary satellite
mission
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air quality; Ozone; Kalman filter; Assimilation; Remote sensing
ID TROPOSPHERIC OZONE; MONITORING INSTRUMENT; POLLUTION INFLUENCES;
UNITED-STATES; CHEMISTRY; PROFILES; MODELS; TES
AB We conduct an Observing System Simulation Experiment (OSSE) to test the ability of geostationary satellite measurements of ozone in different spectral regions to constrain surface ozone concentrations through data assimilation. Our purpose is to define instrument requirements for the NASA GEO-CAPE geostationary air quality mission over North America. We consider instruments using different spectral combinations of UV (290-340 nm), Vis (560-620 nm), and thermal IR (TIR, 9.6 mu m). Hourly ozone data from the MOZART global 3-D chemical transport model (CTM) are taken as the "true" atmosphere to be sampled by the instruments for July 2001. The resulting synthetic data are assimilated in the GEOS-Chem CTM using a Kalman filter. The MOZART and GEOS-Chem CTMs have independent heritages and use different assimilated meteorological data sets for the same period, making for an objective OSSE. We show that hourly observations of ozone from geostationary orbit improve the assimilation considerably relative to daily observation from low earth orbit, and that broad observation over the ocean is unnecessary if the objective is to constrain surface ozone distribution over land. We also show that there is little propagation of ozone information from the free troposphere to the surface, so that instrument sensitivity in the boundary layer is essential. UV + Vis and UV + TIR spectral combinations improve greatly the information on surface ozone relative to UV alone. UV + TIR is preferable under high-sensitivity conditions with strong thermal contrast at the surface, but UV + Vis is preferable under low-sensitivity conditions. Assimilation of data from a UV + Vis + TIR instrument reduces the GEOS-Chem error for surface ozone by a factor of two. Observation in the TIR is critical to obtain ozone information in the upper troposphere relevant to climate forcing. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Zoogman, Peter; Jacob, Daniel J.; Zhang, Lin] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Jacob, Daniel J.; Le Sager, Philippe] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Chance, Kelly; Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fiore, Arlene M.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Eldering, Annmarie; Natraj, Vijay; Kulawik, Susan S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Zoogman, P (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
EM zoogman@fas.harvard.edu
RI Zhang, Lin/A-6729-2008; Chem, GEOS/C-5595-2014; Zhang, Lin/H-9801-2014;
Liu, Xiong/P-7186-2014;
OI Zhang, Lin/0000-0003-2383-8431; Liu, Xiong/0000-0003-2939-574X; Zoogman,
Peter/0000-0002-8848-4999; Chance, Kelly/0000-0002-7339-7577
FU NASA; NASA Earth Science Division, Flight Directorate
FX This work was supported by the NASA Atmospheric Composition and Modeling
Program, by the NASA Earth Science Division, Flight Directorate, and by
a NASA Earth and Space Science Fellowship to Peter Zoogman.
NR 36
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U1 3
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD DEC
PY 2011
VL 45
IS 39
BP 7143
EP 7150
DI 10.1016/j.atmosenv.2011.05.058
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 862UU
UT WOS:000298120400016
ER
PT J
AU Natraj, V
Liu, X
Kulawik, S
Chance, K
Chatfield, R
Edwards, DP
Eldering, A
Francis, G
Kurosu, T
Pickering, K
Spurr, R
Worden, H
AF Natraj, Vijay
Liu, Xiong
Kulawik, Susan
Chance, Kelly
Chatfield, Robert
Edwards, David P.
Eldering, Annmarie
Francis, Gene
Kurosu, Thomas
Pickering, Kenneth
Spurr, Robert
Worden, Helen
TI Multi-spectral sensitivity studies for the retrieval of tropospheric and
lowermost tropospheric ozone from simulated clear-sky GEO-CAPE
measurements
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Multi-spectral; Ozone; Retrieval; Sensitivity; Troposphere;
Geostationary platform; GEO-CAPE
ID MOLECULAR SPECTROSCOPIC DATABASE; RADIATIVE-TRANSFER; MONITORING
INSTRUMENT; PROFILE RETRIEVALS; NADIR RETRIEVALS; AIR-QUALITY;
SATELLITE; POLARIZATION; TES; OBJECTIVES
AB One of the important science requirements of the Geostationary Coastal and Air Pollution Events (GEO-CAPE) mission is to be able to measure ozone with two degrees of freedom in the troposphere and sensitivity in the lowest 2 km (lowermost troposphere, LMT), in order to characterize air quality and boundary layer transport of pollution. Currently available remote sensing techniques utilize backscattered solar ultraviolet (UV) radiances or thermal infrared (TIR) emissions to perform ozone retrievals. However, in the TIR, measurement sensitivity to the LMT requires high thermal contrast between the Earth's surface and the near-surface (tens to hundreds of meters above surface) atmosphere, while in the UV, the measurement sensitivity to the LMT is low because of Rayleigh scattering. In this paper, we explore the feasibility of using multi-spectral intensity measurements in the UV, visible (VIS), mid infrared (MIR) and TIR, and polarization measurements in the UV/VIS, to improve tropospheric and lowermost tropospheric ozone retrievals.
Simulations for 16 cloud and aerosol free atmospheric profiles spanning a range of ozone mixing ratios indicate that adding VIS measurements to UV measurements significantly enhances the sensitivity to lowermost tropospheric ozone, but only makes a slight improvement to the total degrees of freedom for signal (DFS). On the other hand, the combination of UV and TIR significantly improves the total DFS as well as the lowermost tropospheric DFS.
The analysis presented here is a necessary and important first step for defining spectral regions that can meet the GEO-CAPE measurement requirements, and subsequently, the requirements for instrumentation. In this work, the principle of multi-spectral retrievals has been extended from previously published literature and we show that the UV + VIS, UV + TIR and UV + VIS + TIR combinations have the potential to meet the GEO-CAPE measurement requirements for tropospheric ozone. Our analysis includes errors from water and surface properties: further analysis is needed to include temperature, additional gas interferents, clouds, aerosols and more realistic surface properties. These simulations must be run on a much larger dataset, followed by OSSEs (Observing System Simulation Experiments), where simulated retrievals are assimilated into chemical-transport models, to quantitatively assess the impact of the proposed measurements for constraining the spatiotemporal distribution of ozone in the LMT for basic science studies and applications such as air quality forecasts. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Natraj, Vijay; Kulawik, Susan; Eldering, Annmarie; Kurosu, Thomas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chatfield, Robert] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Edwards, David P.; Francis, Gene; Worden, Helen] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Pickering, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Spurr, Robert] RT Solut Inc, Cambridge, MA 02138 USA.
RP Natraj, V (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Vijay.Natraj@jpl.nasa.gov
RI Pickering, Kenneth/E-6274-2012; Liu, Xiong/P-7186-2014;
OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577
FU Earth Science Division of the NASA Science Mission Directorate; Aura OMI
project; National Science Foundation
FX A portion of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology. Funding for this effort was provided
by the Earth Science Division of the NASA Science Mission Directorate.
X.L. was funded by the Aura OMI project. The National Center for
Atmospheric Research is sponsored by the National Science Foundation.
The authors would like to thank the two anonymous reviewers for their
insightful suggestions that undoubtedly improved the quality of the
paper.
NR 89
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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 DEC
PY 2011
VL 45
IS 39
BP 7151
EP 7165
DI 10.1016/j.atmosenv.2011.09.014
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 862UU
UT WOS:000298120400017
ER
PT J
AU Fisher, JA
Jacob, DJ
Wang, QQ
Bahreini, R
Carouge, CC
Cubison, MJ
Dibb, JE
Diehl, T
Jimenez, JL
Leibensperger, EM
Lu, ZF
Meinders, MBJ
Pye, HOT
Quinn, PK
Sharma, S
Streets, DG
van Donkelaar, A
Yantosca, RM
AF Fisher, Jenny A.
Jacob, Daniel J.
Wang, Qiaoqiao
Bahreini, Roya
Carouge, Claire C.
Cubison, Michael J.
Dibb, Jack E.
Diehl, Thomas
Jimenez, Jose L.
Leibensperger, Eric M.
Lu, Zifeng
Meinders, Marcel B. J.
Pye, Havala O. T.
Quinn, Patricia K.
Sharma, Sangeeta
Streets, David G.
van Donkelaar, Aaron
Yantosca, Robert M.
TI Sources, distribution, and acidity of sulfate-ammonium aerosol in the
Arctic in winter-spring
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Arctic; Aerosol acidity; Sulfate; Ammonium; Pollution sources
ID CIRCULATION MODEL ASSESSMENT; CLOUD RESOLVING SIMULATIONS; DRY
DEPOSITION; CHEMICAL-COMPOSITION; ASIAN POLLUTION; ICE NUCLEATION;
AIR-POLLUTION; INTEX-B; ATMOSPHERIC TRANSPORT; OZONE DEPLETION
AB We use GEOS-Chem chemical transport model simulations of sulfate-ammonium aerosol data from the NASA ARCTAS and NOAA ARCPAC aircraft campaigns in the North American Arctic in April 2008, together with longer-term data from surface sites, to better understand aerosol sources in the Arctic in winter-spring and the implications for aerosol acidity. Arctic pollution is dominated by transport from mid-latitudes, and we test the relevant ammonia and sulfur dioxide emission inventories in the model by comparison with wet deposition flux data over the source continents. We find that a complicated mix of natural and anthropogenic sources with different vertical signatures is responsible for sulfate concentrations in the Arctic. East Asian pollution influence is weak in winter but becomes important in spring through transport in the free troposphere. European influence is important at all altitudes but never dominant. West Asia (non-Arctic Russia and Kazakhstan) is the largest contributor to Arctic sulfate in surface air in winter, reflecting a southward extension of the Arctic front over that region. Ammonium in Arctic spring mostly originates from anthropogenic sources in East Asia and Europe, with added contribution from boreal fires, resulting in a more neutralized aerosol in the free troposphere than at the surface. The ARCMS and ARCPAC data indicate a median aerosol neutralization fraction [NH4+]/(2[SO42-] + [NO3-]) of 0.5 mol mol(-1) below 2 km and 0.7 mol mol(-1) above. We find that East Asian and European aerosol transported to the Arctic is mostly neutralized, whereas West Asian and North American aerosol is highly acidic. Growth of sulfur emissions in West Asia may be responsible for the observed increase in aerosol acidity at Barrow over the past decade. As global sulfur emissions decline over the next decades, increasing aerosol neutralization in the Arctic is expected, potentially accelerating Arctic warming through indirect radiative forcing and feedbacks. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Fisher, Jenny A.; Jacob, Daniel J.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Jacob, Daniel J.; Wang, Qiaoqiao; Carouge, Claire C.; Leibensperger, Eric M.; Yantosca, Robert M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Bahreini, Roya; Cubison, Michael J.; Jimenez, Jose L.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Bahreini, Roya] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA.
[Cubison, Michael J.; Jimenez, Jose L.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Dibb, Jack E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Dibb, Jack E.] Univ New Hampshire, Dept Earth Sci, Durham, NH 03824 USA.
[Diehl, Thomas] Univ Space Res Assoc, Columbia, MD USA.
[Diehl, Thomas] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lu, Zifeng; Streets, David G.] Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA.
[Meinders, Marcel B. J.] Univ Wageningen & Res Ctr, Wageningen, Netherlands.
[Pye, Havala O. T.] CALTECH, Dept Chem Engn, Pasadena, CA 91125 USA.
[Quinn, Patricia K.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
[Sharma, Sangeeta] Environm Canada, Div Climate Res, Downsview, ON, Canada.
[van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
RP Fisher, JA (reprint author), Harvard Univ, Dept Earth & Planetary Sci, Pierce Hall G3H,29 Oxford St, Cambridge, MA 02138 USA.
EM jafisher@fas.harvard.edu
RI Jimenez, Jose/A-5294-2008; Pye, Havala/F-5392-2012; Lu,
Zifeng/F-3266-2012; Fisher, Jenny/J-3979-2012; Chem, GEOS/C-5595-2014;
Yantosca, Robert/F-7920-2014; Wang, Qiaoqiao/M-3884-2016; Quinn,
Patricia/R-1493-2016; Manager, CSD Publications/B-2789-2015;
OI Jimenez, Jose/0000-0001-6203-1847; Pye, Havala/0000-0002-2014-2140;
Fisher, Jenny/0000-0002-2921-1691; Yantosca, Robert/0000-0003-3781-1870;
Quinn, Patricia/0000-0003-0337-4895; Streets, David/0000-0002-0223-1350;
Carouge, Claire/0000-0002-0313-8385
FU NASA; U.S. National Science Foundation
FX This work was supported by the NASA Tropospheric Chemistry Program and
the Decadal and Regional Climate Prediction using Earth System Models
(EaSM) Program of the U.S. National Science Foundation. We thank A. M.
Middlebrook for obtaining the ARCPAC AMS data.
NR 131
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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 DEC
PY 2011
VL 45
IS 39
BP 7301
EP 7318
DI 10.1016/j.atmosenv.2011.08.030
PG 18
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 862UU
UT WOS:000298120400032
ER
PT J
AU Ziemba, LD
Griffin, RJ
Whitlow, S
Talbot, RW
AF Ziemba, L. D.
Griffin, R. J.
Whitlow, S.
Talbot, R. W.
TI Characterization of water-soluble organic aerosol in coastal New
England: Implications of variations in size distribution
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Particle size distribution; Water-soluble organic carbon; AIRMAP;
Nuclear magnetic resonance spectroscopy; Carboxylic acid
ID DICARBOXYLIC-ACIDS; ATMOSPHERIC PARTICLES; AROMATIC-HYDROCARBONS;
ELEMENTAL CARBON; HUMIC-LIKE; URBAN; CHROMATOGRAPHY; ISOPRENE; EXHAUST;
MODE
AB Size distributions up to 10-micron aerosol diameter (D-p) of organic carbon (OC) and water-soluble organic carbon (WSOC) were measured at two sites in coastal New England, slightly inland at Thompson Farm (IF) and offshore at Isles of Shoals (IOS). Significant OC concentrations were measured across the full size distribution at IF and IOS, respectively. The WSOC fraction (WSOC/OC) was largest in the accumulation mode with values of 0.86 and 0.93 and smallest in the coarse mode with values of 0.61 and 0.79 at TF and IOS, respectively. Dicarboxylic acids containing up to five carbon atoms (C-s) were concentrated in droplet and accumulation mode aerosol with only minor contributions in the coarse mode. C-1-C-3 monocarboxylic acids were generally near or below detection limits. Results from proton nuclear magnetic resonance (H+-NMR) spectroscopy analyses showed that the organic functional group characterized by protons in the alpha position to an unsaturated carbon atoms ([H-C-C=]) was the dominant WSOC functionality at both TF and IOS, constituting 34 and 43% of carbon-weighted H+-NMR signal, respectively. Size distributions of each H+-NMR-resolved organic functionality are presented. Source apportionment using H+-NMR fingerprints is also presented, and results indicate that nearly all of the WSOC at IF and IOS spectroscopically resembled secondary organic aerosol, regardless of D-P. Published by Elsevier Ltd.
C1 [Ziemba, L. D.; Griffin, R. J.; Whitlow, S.; Talbot, R. W.] Univ New Hampshire, Climate Change Res Ctr, Durham, NH 03824 USA.
RP Ziemba, LD (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM luke.ziemba@nasa.gov
FU NOAA Office of Oceanic and Atmospheric Research [NA07OAR4600514,
NA06OAR4600189]
FX Financial support was from the NOAA Office of Oceanic and Atmospheric
Research under grants #NA07OAR4600514 and #NA06OAR4600189. Thanks to
Casey Anderson and Chelsea Corr and the staff at Appledore Island for
logistical support. Special thanks to Patricia Wilkinson at the
University Instrumentation Center at UNH for training and use of the NRM
instrument and facility.
NR 56
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U2 23
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 DEC
PY 2011
VL 45
IS 39
BP 7319
EP 7329
DI 10.1016/j.atmosenv.2011.08.022
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 862UU
UT WOS:000298120400033
ER
PT J
AU Bradley, ES
Roberts, DA
Dennison, PE
Green, RO
Eastwood, M
Lundeen, SR
McCubbin, IB
Leifer, I
AF Bradley, Eliza S.
Roberts, Dar A.
Dennison, Philip E.
Green, Robert O.
Eastwood, Michael
Lundeen, Sarah R.
McCubbin, Ian B.
Leifer, Ira
TI Google Earth and Google Fusion Tables in support of time-critical
collaboration: Mapping the deepwater horizon oil spill with the AVIRIS
airborne spectrometer
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Remote sensing image database; Airborne imaging spectrometry; Google
Earth; Google Fusion Tables; AVIRIS; Deepwater horizon oil spill
ID WEB 2.0; HYPERSPECTRAL IMAGES; HEALTH; VISUALIZATION; DISPLAY; KOREA
AB Web interfaces have made remote sensing image resources more accessible and interactive. However, many web-based and Digital Earth opportunities for remote sensing have not yet been fully explored and could greatly facilitate scientific collaboration. In many cases, these resources can augment traditional proprietary software packages, which can have limited flexibility, spatiotemporal controls, and data synthesis abilities. In this paper, we discuss how web services and Google Earth were used for time-critical geovisualizations of the NASA Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) Deepwater Horizon oil spill imaging campaign. In particular, we describe how (1) AVIRIS Google Earth products were used to visualize the spatial and temporal characteristics of the campaign's image acquisitions, critically needed for flight planning, (2) the Google Fusion Table cloud-based service was applied to create a highly-interactive image archive and mapping display, and (3) the Google Fusion Table API was utilized to create a flexible PHP-based interface for metadata creation and as the basis for an interactive data catalog. Although there are other possible software and programming approaches to these activities, we highlight freely-accessible and flexible solutions and bring attention to the newly introduced Google Fusion Tables as a collaborative scientific platform.
C1 [Bradley, Eliza S.; Roberts, Dar A.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Dennison, Philip E.] Univ Utah, Dept Geog, Salt Lake City, UT 84112 USA.
[Dennison, Philip E.] Univ Utah, Ctr Nat & Technol Hazards, Salt Lake City, UT 84112 USA.
[Green, Robert O.; Eastwood, Michael; Lundeen, Sarah R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McCubbin, Ian B.] Desert Res Inst, Storm Peak Lab, Steamboat Springs, CO 80488 USA.
[Leifer, Ira] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA.
RP Bradley, ES (reprint author), Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
EM ebradley@geog.ucsb.edu
OI Leifer, Ira/0000-0002-4674-5775; Dennison, Philip/0000-0002-0241-1917
NR 48
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U1 3
U2 40
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD DEC
PY 2011
VL 4
IS 4
SI SI
BP 169
EP 179
DI 10.1007/s12145-011-0085-4
PG 11
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 864HL
UT WOS:000298228600002
ER
PT J
AU Ponchak, GE
AF Ponchak, George E.
TI SPECIAL ISSUE ON 2011 INTERNATIONAL MICROWAVE SYMPOSIUM
SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES
LA English
DT Editorial Material
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9480
J9 IEEE T MICROW THEORY
JI IEEE Trans. Microw. Theory Tech.
PD DEC
PY 2011
VL 59
IS 12
SI SI
BP 3263
EP 3263
DI 10.1109/TMTT.2011.2173512
PN 2
PG 1
WC Engineering, Electrical & Electronic
SC Engineering
GA 861WX
UT WOS:000298052000001
ER
PT J
AU Nikolic, M
Popovic, S
Vuskovic, L
Herring, GC
Exton, RJ
AF Nikolic, M.
Popovic, S.
Vuskovic, L.
Herring, G. C.
Exton, R. J.
TI Electron density measurements in a pulse-repetitive microwave discharge
in air
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID SPECTROSCOPIC DIAGNOSTICS; NITROGEN; PRESSURE; PLASMAS; PARAMETERS;
EXCITATION
AB We have developed a technique for absolute measurements of electron density in pulse-repetitive microwave discharges in air. The technique is based on the time-resolved absolute intensity of a nitrogen spectral band belonging to the Second Positive System, the kinetic model and the detailed particle balance of the N(2)C(3)Pi(u) (v = 0) state. This new approach bridges the gap between two existing electron density measurement methods (Langmuir probe and Stark broadening). The electron density is obtained from the time-dependent rate equation for the population of N(2)C(3)Pi(u) (v = 0) using recorded waveforms of the absolute C(3)Pi(u) -> B(3)Pi(g) (0-0) band intensity, the forward and reflected microwave power density. Measured electron density waveforms using numerical and approximated analytical methods are presented for the case of pulse repetitive planar surface microwave discharge at the aperture of a horn antenna covered with alumina ceramic plate. The discharge was generated in air at 11.8 Torr with a X-band microwave generator using 3.5 mu s microwave pulses at peak power of 210 kW. In this case, we were able to time resolve the electron density within a single 3.5 mu s pulse. We obtained (9.0 +/- 0.6) x 10(13) cm(-3) for the peak and (5.0 +/- 0.6) x 10(13) cm(-3) for the pulse-average electron density. The technique presents a convenient, non-intrusive diagnostic method for local, time-defined measurements of electron density in short duration discharges near atmospheric pressures. (C) 2011 American Institute of Physics. [doi: 10.1063/1.3665195]
C1 [Nikolic, M.; Popovic, S.; Vuskovic, L.] Old Dominion Univ, Dept Phys, Ctr Accelerator Sci, Norfolk, VA 23529 USA.
[Herring, G. C.; Exton, R. J.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Nikolic, M (reprint author), Old Dominion Univ, Dept Phys, Ctr Accelerator Sci, Norfolk, VA 23529 USA.
EM mniko004@odu.edu
NR 19
TC 1
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U1 3
U2 7
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD DEC 1
PY 2011
VL 110
IS 11
AR 113304
DI 10.1063/1.3665195
PG 7
WC Physics, Applied
SC Physics
GA 864QL
UT WOS:000298254800019
ER
PT J
AU Hilker, T
Coops, NC
Gaulton, R
Wulder, MA
Cranston, J
Stenhouse, G
AF Hilker, Thomas
Coops, Nicholas C.
Gaulton, Rachel
Wulder, Michael A.
Cranston, Jerome
Stenhouse, Gordon
TI Biweekly disturbance capture and attribution: case study in western
Alberta grizzly bear habitat
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE disturbance mapping; disturbance attribution; Landsat; MODIS; change
detection; temporal resolution; forest harvest; Ursus arctos L.
ID REFLECTANCE FUSION MODEL; LANDSAT DATA; FOREST; CANADA; SELECTION
AB An increasing number of studies have demonstrated the impact of landscape disturbance on ecosystems. Satellite remote sensing can be used for mapping disturbances, and fusion techniques of sensors with complimentary characteristics can help to improve the spatial and temporal resolution of satellite-based mapping techniques. Classification of different disturbance types from satellite observations is difficult, yet important, especially in an ecological context as different disturbance types might have different impacts on vegetation recovery, wildlife habitats, and food resources. We demonstrate a possible approach for classifying common disturbance types by means of their spatial characteristics. First, landscape level change is characterized on a near biweekly basis through application of a data fusion model (spatial temporal adaptive algorithm for mapping reflectance change) and a number of spatial and temporal characteristics of the predicted disturbance patches are inferred. A regression tree approach is then used to classify disturbance events. Our results show that spatial and temporal disturbance characteristics can be used to classify disturbance events with an overall accuracy of 86% of the disturbed area observed. The date of disturbance was identified as the most powerful predictor of the disturbance type, together with the patch core area, patch size, and contiguity. (C) 2011 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.3664342]
C1 [Hilker, Thomas] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Coops, Nicholas C.] Univ British Columbia, Fac Forest Resources Management, Vancouver, BC V6T 1Z4, Canada.
[Gaulton, Rachel] Newcastle Univ, Dept Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Wulder, Michael A.] Canadian Forest Serv, Pacific Forestry Ctr, Nat Resources Canada, Victoria, BC V8Z 1M5, Canada.
[Cranston, Jerome; Stenhouse, Gordon] Foothills Res Inst, Hinton, AB T7V 1X6, Canada.
RP Hilker, T (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 618, Greenbelt, MD 20771 USA.
EM thomas.hilker@nasa.gov
RI Coops, Nicholas/J-1543-2012; Wulder, Michael/J-5597-2016
OI Coops, Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896
FU Foothills Research Institute located in Hinton, Alberta, Canada; NSERC
through the Canadian Forest Service (CFS)
FX Funding for this research was generously provided by the Grizzly Bear
Program of the Foothills Research Institute located in Hinton, Alberta,
Canada, with additional information available at: http://www.fmf.ab.ca/.
Additional funding provided through an NSERC grant to Coops, and to
Wulder through the Canadian Forest Service (CFS).
NR 28
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U1 0
U2 13
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 DEC 1
PY 2011
VL 5
AR 053568
DI 10.1117/1.3664342
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 866HV
UT WOS:000298372200001
ER
PT J
AU Bilitza, D
McKinnell, LA
Reinisch, B
Fuller-Rowell, T
AF Bilitza, Dieter
McKinnell, Lee-Anne
Reinisch, Bodo
Fuller-Rowell, Tim
TI The international reference ionosphere today and in the future
SO JOURNAL OF GEODESY
LA English
DT Review
DE Ionosphere; IRI; Empirical model; F2 peak models; Topside
ID ELECTRON-DENSITY PROFILES; AURORAL OVAL BOUNDARIES; EMPIRICAL-MODEL;
IONOSONDE MEASUREMENTS; TOPSIDE IONOSPHERE; RADIO OCCULTATION; SCALE
HEIGHT; IRI MODEL; IONOGRAMS; SPECIFICATION
AB The international reference ionosphere (IRI) is the internationally recognized and recommended standard for the specification of plasma parameters in Earth's ionosphere. It describes monthly averages of electron density, electron temperature, ion temperature, ion composition, and several additional parameters in the altitude range from 60 to 1,500 km. A joint working group of the Committee on Space Research (COSPAR) and the International Union of Radio Science (URSI) is in charge of developing and improving the IRI model. As requested by COSPAR and URSI, IRI is an empirical model being based on most of the available and reliable data sources for the ionospheric plasma. The paper describes the latest version of the model and reviews efforts towards future improvements, including the development of new global models for the F2 peak density and height, and a new approach to describe the electron density in the topside and plasmasphere. Our emphasis will be on the electron density because it is the IRI parameter most relevant to geodetic techniques and studies. Annual IRI meetings are the main venue for the discussion of IRI activities, future improvements, and additions to the model. A new special IRI task force activity is focusing on the development of a real-time IRI (RT-IRI) by combining data assimilation techniques with the IRI model. A first RT-IRI task force meeting was held in 2009 in Colorado Springs. We will review the outcome of this meeting and the plans for the future. The IRI homepage is at http://www.IRI.gsfc.nasa.gov.
C1 [Bilitza, Dieter] George Mason Univ, Space Weather Lab, Fairfax, VA 22030 USA.
[Bilitza, Dieter] NASA, Goddard Space Flight Ctr, Heliospher Lab, Greenbelt, MD 20771 USA.
[McKinnell, Lee-Anne] Hermanus Magnet Observ, ZA-7200 Hermanus, South Africa.
[Reinisch, Bodo] Univ Massachusetts, Ctr Atmospher Res, Lowell, MA 01854 USA.
[Fuller-Rowell, Tim] Univ Colorado, CIRES, Boulder, CO 80305 USA.
[Fuller-Rowell, Tim] NOAA, Space Weather Predict Ctr, Boulder, CO 80305 USA.
RP Bilitza, D (reprint author), George Mason Univ, Space Weather Lab, Fairfax, VA 22030 USA.
EM dbilitza@gmu.edu; lmckinnell@hmo.ac.za; Bodo_Reinisch@uml.edu;
Tim.Fuller-Rowell@noaa.gov
FU NSF [ATM-0819440]; NASA [NNX09AJ74G, NNX07-AG38G, NNX07AO65G]
FX We acknowledge the contributions of IRI Working Group members to the IRI
effort and the many users of the model who have provided valuable
feedback. This work was supported through NSF grant ATM-0819440 and NASA
Grants NNX09AJ74G, NNX07-AG38G, and NNX07AO65G.
NR 80
TC 130
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U1 2
U2 23
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 DEC
PY 2011
VL 85
IS 12
SI SI
BP 909
EP 920
DI 10.1007/s00190-010-0427-x
PG 12
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 869HB
UT WOS:000298587700003
ER
PT J
AU Lee, CK
Han, SC
Bilitza, D
Chung, JK
AF Lee, Choon-Ki
Han, Shin-Chan
Bilitza, Dieter
Chung, Jong-Kyun
TI Validation of international reference ionosphere models using in situ
measurements from GRACE K-band ranging system and CHAMP planar Langmuir
probe
SO JOURNAL OF GEODESY
LA English
DT Article
DE Ionosphere; Electron density; GRACE; CHAMP; IRI
ID TOPSIDE ELECTRON-DENSITY; SOLAR-ACTIVITY; IRI; PREDICTIONS
AB The in situ measurements of electron contents from GRACE K-band (dual-frequency) ranging system and CHAMP planar Langmuir probe were used to validate the international reference ionosphere (IRI) models. The comparison using measurements from year 2003 to 2007 shows a general agreement between data and the model outputs. The improvement in the newer IRI model (IRI-2007) is evident with the measurements from the GRACE satellites orbiting at the higher altitude. We present the comparison between the models and data comprehensively for various cases in solar activity, local time, season, and latitude. The IRI models do not well predict the electron density in the years 2006 and later, when the solar activity is extremely low. The IRI models generally overestimate the electron density during local winter while they underestimate during local summer. In the equatorial region, the large difference at local sunrise lasts for all years and all seasons. The IRI models do not perform well in predicting the anomaly in the polar region such as the Weddell Sea Anomaly. These discrepancies are likely due to smoothed (12-month averaged) solar activity indices used in the IRI models and due to insufficient spherical harmonic representation not able to capture small spatial scales. In near future, further improvement on the IRI models is expected by assimilating those in situ satellite data by implementing higher resolution (spatial and temporal) parameterizations.
C1 [Lee, Choon-Ki; Han, Shin-Chan] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Lee, Choon-Ki; Han, Shin-Chan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Bilitza, Dieter] NASA, Goddard Space Flight Ctr, Heliophys Lab, Greenbelt, MD USA.
[Bilitza, Dieter] George Mason Univ, Fairfax, VA 22030 USA.
[Chung, Jong-Kyun] Korea Astron & Space Sci Inst, Space Geodesy Res Div, Taejon, South Korea.
RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA.
EM shin-chan.han@nasa.gov
RI Han, Shin-Chan/A-2022-2009
FU NASA GRACE; Earth Surface and Interior program; Korea Meteorological
Administration [CATER 2008-5406]
FX This work was supported by NASA GRACE project and Earth Surface and
Interior program. We would like to thank the German Space Operations
Center of the German Aerospace Center, DLR, for providing continuously
and nearly 100% of the raw telemetry data of the twin GRACE satellites
and JPL for producing the high-quality Level-1B products. The
constructive comments from two anonymous reviewers and Michael Schmidt
greatly helped to improve the original manuscript. CKL was also
supported by the Korea Meteorological Administration Research and
Development Program under CATER 2008-5406.
NR 23
TC 5
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U1 1
U2 1
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 DEC
PY 2011
VL 85
IS 12
SI SI
BP 921
EP 929
DI 10.1007/s00190-011-0442-6
PG 9
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 869HB
UT WOS:000298587700004
ER
PT J
AU Banks, HT
Cioranescu, D
Criner, AK
Winfree, WP
AF Banks, H. T.
Cioranescu, D.
Criner, A. K.
Winfree, W. P.
TI Parameter estimation for the heat equation on perforated domains
SO JOURNAL OF INVERSE AND ILL-POSED PROBLEMS
LA English
DT Article
DE Inverse problems; parameter estimation; perforated domains;
homogenization; thermal diffusion; ordinary least squares; generalized
least squares
AB In this effort we investigate the behavior of a model derived from homogenization theory as the model solution in parameter estimation procedures for simulated data for heat flow in a porous medium. We consider data simulated from a model on a perforated domain with isotropic flow and data simulated from a model on a homogeneous domain with anisotropic flow. We report on both ordinary and generalized least squares parameter estimation procedures.
C1 [Banks, H. T.; Criner, A. K.] N Carolina State Univ, Dept Math, Ctr Res Sci Computat, Raleigh, NC 27695 USA.
[Cioranescu, D.] Univ Paris 06, Lab JL Lions, F-75005 Paris, France.
[Winfree, W. P.] NASA Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA.
RP Banks, HT (reprint author), N Carolina State Univ, Dept Math, Ctr Res Sci Computat, Box 8205, Raleigh, NC 27695 USA.
FU National Science Foundation [DMS-0636590]; Air Force Office of
Scientific Research [FA9550-09-1-0226]
FX This research was supported in part by the National Science Foundation
under Research Training Grant (RTG) DMS-0636590 and in part by the Air
Force Office of Scientific Research under grant number FA9550-09-1-0226.
NR 21
TC 1
Z9 1
U1 0
U2 3
PU WALTER DE GRUYTER GMBH
PI BERLIN
PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY
SN 0928-0219
EI 1569-3945
J9 J INVERSE ILL-POSE P
JI J. Inverse Ill-Posed Probl.
PD DEC
PY 2011
VL 19
IS 6
BP 825
EP 857
DI 10.1515/JIIP.2011.051
PG 33
WC Mathematics, Applied; Mathematics
SC Mathematics
GA 862UI
UT WOS:000298119200002
ER
PT J
AU Li, LM
Jiang, X
Chahine, MT
Wang, JQ
Yung, YL
AF Li, Liming
Jiang, Xun
Chahine, Moustafa T.
Wang, Jingqian
Yung, Yuk L.
TI The Mechanical Energies of the Global Atmosphere in El Nino and La Nina
Years
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID SURFACE-TEMPERATURE; GENERAL CIRCULATION; PLANETARY SCALE; CYCLE;
ENERGETICS; REANALYSIS; MODELS
AB Two meteorological reanalysis datasets are analyzed to determine the mechanical energies of the global atmosphere in the El Nino and La Nina years. The general consistency of the mean energy components between the two datasets reveals similar to 1%-3% increase and similar to 2%-3% decrease in the mean energies in the El Nino years and La Nina years, respectively. These analyses further reveal that the tropospheric temperature responds to the sea surface temperature anomaly with a time lag of two months, which leads to the varying mean atmospheric energies in the El Nino and La Nina years.
C1 [Li, Liming; Jiang, Xun; Wang, Jingqian] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
[Chahine, Moustafa T.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA USA.
[Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Li, LM (reprint author), Univ Houston, Dept Earth & Atmospher Sci, 312 Sci & Res Bldg 1,Rm 312, Houston, TX 77204 USA.
EM lli7@mail.uh.edu
FU Jet Propulsion Laboratory, California Institute of Technology under
National Aeronautics and Space Administration (NASA); NASA
FX We thank M. Gerstell for helpful comments. This work was partly
supported by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration (NASA). This work is also supported by NASA Outer Planets
Research Program.
NR 26
TC 2
Z9 2
U1 0
U2 0
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 DEC
PY 2011
VL 68
IS 12
BP 3072
EP 3078
DI 10.1175/JAS-D-11-072.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 863YY
UT WOS:000298205400017
ER
PT J
AU Marshak, A
Knyazikhin, Y
Chiu, JC
Wscombe, WJ
AF Marshak, A.
Knyazikhin, Y.
Chiu, J. C.
Wscombe, W. J.
TI Spectrally Invariant Approximation within Atmospheric Radiative Transfer
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID DISCRETE-ORDINATE-METHOD; LEAF-AREA INDEX; SOLAR-RADIATION;
HYPERSPECTRAL DATA; VEGETATION; CLOUDS; PARAMETERIZATION; ABSORPTION;
ALGORITHM; CANOPIES
AB Certain algebraic combinations of single scattering albedo and solar radiation reflected from, or transmitted through, vegetation canopies do not vary with wavelength. These "spectrally invariant relationships" are the consequence of wavelength independence of the extinction coefficient and scattering phase function in vegetation. In general, this wavelength independence does not hold in the atmosphere, but in cloud-dominated atmospheres the total extinction and total scattering phase function vary only weakly with wavelength. This paper identifies the atmospheric conditions under which the spectrally invariant approximation can accurately describe the extinction and scattering properties of cloudy atmospheres. The validity of the assumptions and the accuracy of the approximation are tested with 1D radiative transfer calculations using publicly available radiative transfer models: Discrete Ordinate Radiative Transfer (DISORT) and Santa Barbara DISORT Atmospheric Radiative Transfer (SBDART). It is shown for cloudy atmospheres with cloud optical depth above 3, and for spectral intervals that exclude strong water vapor absorption, that the spectrally invariant relationships found in vegetation canopy radiative transfer are valid to better than 5%. The physics behind this phenomenon, its mathematical basis, and possible applications to remote sensing and climate are discussed.
C1 [Marshak, A.; Wscombe, W. J.] NASA, Climate & Radiat Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Knyazikhin, Y.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Chiu, J. C.] Univ Reading, Dept Meteorol, Reading, Berks, England.
RP Marshak, A (reprint author), NASA, Climate & Radiat Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM alexander.marshak@nasa.gov
RI Chiu, Christine/E-5649-2013; Marshak, Alexander/D-5671-2012
OI Chiu, Christine/0000-0002-8951-6913;
FU Office of Science (BER, U.S. Department of Energy) [DE-AI02-08ER64562,
DE-FG02-08ER64563, DE-FG02-08ER54564]
FX This research was supported by the Office of Science (BER, U.S.
Department of Energy, Interagency Agreements DE-AI02-08ER64562,
DE-FG02-08ER64563, and DE-FG02-08ER54564) as part of the ARM program. We
also thank A. Davis, F. Evans, A. Lyapustin, L. Oreopoulos, P.
Pilewskie, R. Pincus, S. Schmidt, A. Vasilkov, and Z. Zhang for fruitful
discussions.
NR 27
TC 3
Z9 4
U1 0
U2 4
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 DEC
PY 2011
VL 68
IS 12
BP 3094
EP 3111
DI 10.1175/JAS-D-11-060.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 863YY
UT WOS:000298205400019
ER
PT J
AU Kandula, M
AF Kandula, M.
TI Sound Radiation from a Supersonic Jet Passing Through a Partially Open
Exhaust Duct
SO JOURNAL OF VIBRATION AND ACOUSTICS-TRANSACTIONS OF THE ASME
LA English
DT Article
DE Sound emission; jet noise; ducted exhaust
ID HIGH-SPEED JET; NOISE-REDUCTION; WATER INJECTION
AB The radiation of sound from a perfectly expanded Mach 2.5 cold supersonic jet of 25.4 mm exit diameter flowing through a partially open rigid-walled duct with an upstream J-deflector has been experimentally studied. In the experiments, the nozzle is mounted vertically, with the nozzle exit plane at a height of 73 jet diameters above ground level. Relative to the nozzle exit plane (NEP), the location of the duct inlet is varied at 10, 5, and -1 jet diameters. Far-field sound pressure levels were obtained at 54 jet diameters above ground with the aid of acoustic sensors equally spaced around a circular arc of radius equal to 80 jet diameters from the jet axis. Data on the jet acoustic field for the partially open duct were obtained and compared with those with a free jet and with a closed duct. The results suggest that for the partially open duct the overall sound pressure level (OASPL) decreases as the distance between the NEP and the duct inlet plane decreases, while the opposite trend is observed for the closed duct. It is also concluded that the observed peak frequency in the partially open duct increases above the free jet value as the angle from the duct axis is increased, and as the duct inlet plane becomes closer to the NEP. [DOI: 10.1115/1.4004671]
C1 NASA, ASRC Aerosp, Kennedy Space Ctr, FL 32899 USA.
RP Kandula, M (reprint author), NASA, ASRC Aerosp, Kennedy Space Ctr, FL 32899 USA.
EM max.kandula-1@nasa.gov
NR 23
TC 0
Z9 0
U1 2
U2 3
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 1048-9002
J9 J VIB ACOUST
JI J. Vib. Acoust.-Trans. ASME
PD DEC
PY 2011
VL 133
IS 6
AR 064503
DI 10.1115/1.4004671
PG 5
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA 861HN
UT WOS:000298010100024
ER
PT J
AU Hallis, LJ
Taylor, GJ
AF Hallis, Lydia J.
Taylor, G. J.
TI Comparisons of the four Miller Range nakhlites, MIL 03346, 090030,
090032 and 090136: Textural and compositional observations of primary
and secondary mineral assemblages
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID MERIDIANI-PLANUM; AQUEOUS ALTERATION; MARS; METEORITES; PHYLLOSILICATES;
ENVIRONMENT; ANTARCTICA; CHEMISTRY; PETROLOGY; ROCKS
AB Petrological and geochemical analyses of Miller Range (MIL) 03346 indicate that this meteorite originated from the same augitic cumulate layer(s) as the nakhlite Martian meteorites, but underwent rapid cooling prior to complete crystallization. As with the other nakhlites, MIL 03346 contains a secondary alteration assemblage, in this case consisting of iddingsite-like alteration veins in olivine phenocrysts, Fe-oxide alteration veins associated with the mesostasis, and Ca- and K,Fe-sulfate veins. We compared the textural and mineralogical compositions of MIL 090030, 090032, and 090136 with MIL 03346, focusing on the composition and Raman spectra of the alteration assemblages. These observations indicate that the meteorites are paired, and that the preterrestrial olivine-bound alteration assemblages were produced by weakly acidic brine. Although these alteration assemblages resemble similar assemblages in Nakhla, the absence of siderite and halite in the Miller Range nakhlites indicates that the parental alteration brine was comparatively HCO3- depleted, and less concentrated, than that which altered Nakhla. This indicates that the Miller Range nakhlite alteration brine experienced a separate evolutionary pathway to that which altered Nakhla, and therefore represents a separate branch of the Lafayette-Nakhla evaporation sequence. Thin-sections cut from the internal portions of these meteorites (away from any fusion crust or terrestrially exposed edge), contain little Ca-sulfate (identified as gypsum), and no jarosite, whereas thin-sections with terrestrially exposed edges have much higher sulfate abundances. These observations suggest that at least the majority of sulfate within the Miller Range nakhlites is terrestrially derived.
C1 [Hallis, Lydia J.; Taylor, G. J.] Univ Hawaii, HIGP SOEST, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Hallis, LJ (reprint author), Univ Hawaii, HIGP SOEST, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
EM lydh@higp.hawaii.edu
FU NASA astrobiology institute
FX We thank the NASA Johnson Space Center for allocation of the Miller
Range nakhlite thin-sections, and Eric Hellebrand for his assistance
with our EMP analyses. We also thank the NASA astrobiology institute for
funding this research. The comments and suggestions of Prof. Allan
Treiman and two anonymous reviewers, as well as Associate Editor Prof.
Christine Floss, were invaluable in improving this manuscript.
NR 57
TC 29
Z9 29
U1 1
U2 12
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD DEC
PY 2011
VL 46
IS 12
BP 1787
EP 1803
DI 10.1111/j.1945-5100.2011.01293.x
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 862MD
UT WOS:000298094600001
ER
PT J
AU Fairen, AG
Dohm, JM
Baker, VR
Thompson, SD
Mahaney, WC
Herkenhoff, KE
Rodriguez, JAP
Davila, AF
Schulze-Makuch, D
El Maarry, MR
Uceda, ER
Amils, R
Miyamoto, H
Kim, KJ
Anderson, RC
McKay, CP
AF Fairen, Alberto G.
Dohm, James M.
Baker, Victor R.
Thompson, Shane D.
Mahaney, William C.
Herkenhoff, Kenneth E.
Rodriguez, J. Alexis P.
Davila, Alfonso F.
Schulze-Makuch, Dirk
El Maarry, M. Ramy
Uceda, Esther R.
Amils, Ricardo
Miyamoto, Hirdy
Kim, Kyeong J.
Anderson, Robert C.
McKay, Christopher P.
TI Meteorites at Meridiani Planum provide evidence for significant amounts
of surface and near-surface water on early Mars
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID TERRESTRIAL AGES; TERRA-MERIDIANI; BURNS FORMATION; CHONDRITE; DEPOSITS;
STRATIGRAPHY; ANTARCTICA; CRATERS; ARABIA; ORIGIN
AB Six large iron meteorites have been discovered in the Meridiani Planum region of Mars by the Mars Exploration Rover Opportunity in a nearly 25 km-long traverse. Herein, we review and synthesize the available data to propose that the discovery and characteristics of the six meteorites could be explained as the result of their impact into a soft and wet surface, sometime during the Noachian or the Hesperian, subsequently to be exposed at the Martian surface through differential erosion. As recorded by its sediments and chemical deposits, Meridiani has been interpreted to have undergone a watery past, including a shallow sea, a playa, an environment of fluctuating ground water, and/or an icy landscape. Meteorites could have been encased upon impact and/or subsequently buried, and kept underground for a long time, shielded from the atmosphere. The meteorites apparently underwent significant chemical weathering due to aqueous alteration, as indicated by cavernous features that suggest differential acidic corrosion removing less resistant material and softer inclusions. During the Amazonian, the almost complete disappearance of surface water and desiccation of the landscape, followed by induration of the sediments and subsequent differential erosion and degradation of Meridiani sediments, including at least 1080 m of deflation in the last 33.5 Gy, would have exposed the buried meteorites. We conclude that the iron meteorites support the hypothesis that Mars once had a denser atmosphere and considerable amounts of water and/or water ice at and/or near the surface.
C1 [Fairen, Alberto G.; Davila, Alfonso F.] SETI Inst, Mountain View, CA 94043 USA.
[Fairen, Alberto G.; Davila, Alfonso F.; Uceda, Esther R.; McKay, Christopher P.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Dohm, James M.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Thompson, Shane D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Mahaney, William C.] Quaternary Surveys, Thornhill, ON L4J 1J4, Canada.
[Herkenhoff, Kenneth E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Rodriguez, J. Alexis P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Schulze-Makuch, Dirk] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99163 USA.
[El Maarry, M. Ramy] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Amils, Ricardo] Ctr Astrobiol INTA CSIC, Madrid 28850, Spain.
[Miyamoto, Hirdy] Univ Tokyo, Tokyo, Japan.
[Kim, Kyeong J.] Korea Inst Geosci & Mineral Resources, Taejon, South Korea.
[Anderson, Robert C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fairen, AG (reprint author), SETI Inst, 189 N Bernardo Ave, Mountain View, CA 94043 USA.
EM alberto.g.fairen@nasa.gov
RI Miyamoto, Hideaki/E-3381-2012; Davila, Alfonso/A-2198-2013; Dohm,
James/A-3831-2014;
OI Davila, Alfonso/0000-0002-0977-9909; EL-MAARRY, MOHAMED
RAMY/0000-0002-8262-0320; Kim, Kyeong J/0000-0001-6220-8411;
Schulze-Makuch, Dirk/0000-0002-1923-9746
NR 52
TC 10
Z9 10
U1 1
U2 16
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD DEC
PY 2011
VL 46
IS 12
BP 1832
EP 1841
DI 10.1111/j.1945-5100.2011.01297.x
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 862MD
UT WOS:000298094600004
ER
PT J
AU Scott, ERD
Bottke, WF
AF Scott, Edward R. D.
Bottke, William F.
TI Impact histories of angrites, eucrites, and their parent bodies
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID MAIN ASTEROID BELT; EARLY SOLAR-SYSTEM; ANGRA-DOS-REIS; SHOCK
METAMORPHISM; DIFFERENTIATED PLANETESIMALS; IRON-METEORITES; THERMAL
HISTORY; BODY; CHONDRITES; VESTA
AB Eucrites, which are probably from 4 Vesta, and angrites are the two largest groups of basaltic meteorites from the asteroid belt. The parent body of the angrites is not known but it may have been comparable in size to Vesta as it retained basalts and had a core dynamo. Both bodies were melted early by 26Al and formed basalts a few Myr after they accreted. Despite these similarities, the impact histories of the angrites and eucrites are very different: angrites are very largely unshocked and none are breccias, whereas most eucrites are breccias and many are shocked. We attribute the lack of shocked and unbrecciated angrites to an impact, possibly at 4558 Myr agothe radiometric age of the younger angritesthat extracted the angrites from their original parent body into smaller bodies. These bodies, which may have had a diameter of approximately 10 km, suffered much less impact damage than Vesta during the late heavy bombardment because small bodies retain shocked rocks less efficiently than large ones and because large bodies suffer near-catastrophic impacts that deposit vastly more impact energy per kg of target. Our proposed history for the angrites is comparable to that proposed by Bogard and Garrison (2003) for the unbrecciated eucrites with Ar-Ar ages of 4.48 Gyr and that for unbrecciated eucrites with anomalous oxygen isotopic compositions that did not come from Vesta. We infer that the original parent bodies of the angrites and the anomalous eucrites were lost from the belt when the giant planets migrated and the total mass of asteroids was severely depleted. Alternatively, their parent bodies may have formed in the terrestrial planet region and fragments of these bodies were scattered out to the primordial Main Belt as a consequence of terrestrial planet formation.
C1 [Scott, Edward R. D.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Bottke, William F.] SW Res Inst, Boulder, CO 80302 USA.
[Bottke, William F.] NASA, Lunar Sci Inst, Boulder, CO 80302 USA.
RP Scott, ERD (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
EM escott@hawaii.edu
FU NASA Cosmochemistry [NNX09AH30G]; NSF [AST0909166]
FX We thank Don Bogard for helpful discussions about the ages and histories
of HED meteorites, Ian Sanders for advice on the radiometric ages and
origins of eucrites and angrites, Klaus Keil for helpful discussions on
angrites, the Smithsonian Institution for the loan of the D'Orbigny thin
section, and Takashi Mikouchi and an anonymous reviewer for their
helpful comments. This work was partly supported by NASA Cosmochemistry
grant NNX09AH30G to ES and NSF Planetary Astronomy grant AST0909166 to
WB.
NR 87
TC 8
Z9 8
U1 2
U2 14
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD DEC
PY 2011
VL 46
IS 12
BP 1878
EP 1887
DI 10.1111/j.1945-5100.2011.01301.x
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 862MD
UT WOS:000298094600007
ER
PT J
AU Campbell, JF
Prasad, NS
Flood, MA
AF Campbell, Joel F.
Prasad, Narasimha S.
Flood, Michael A.
TI Pseudorandom noise code-based technique for thin-cloud discrimination
with CO2 and O-2 absorption measurements
SO OPTICAL ENGINEERING
LA English
DT Article
DE active sensing of CO2 emissions over nights, days, and seasons; CO2
sensing; O-2 sensing; PN codes; CW lidar
ID MODULATION CW LIDAR; SEQUENCES
AB NASA Langley Research Center is working on a continuous wave (cw) laser-based remote sensing scheme for the detection of CO2 and O-2 from space-based platforms suitable for an active sensing of CO2 emissions over nights, days, and seasons (ASCENDS) mission. ASCENDS is a future space-based mission to determine the global distribution of sources and sinks of atmospheric carbon dioxide (CO2). A unique, multifrequency, intensity modulated cw laser absorption spectrometer operating at 1.57 mu m for CO2 sensing has been developed. Effective aerosol and cloud discrimination techniques are being investigated in order to determine concentration values with accuracies less than 0.3%. In this paper, we discuss the demonstration of a pseudonoise code-based technique for cloud and aerosol discrimination applications. The possibility of using maximum length sequences for range and absorption measurements is investigated. A simple model for accomplishing this objective is formulated. Proof-of-concept experiments carried out using a sonar-based LIDAR simulator that was built using simple audio hardware provided promising results for extension into optical wavelengths. (C) 2011 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.3658758]
C1 [Campbell, Joel F.; Prasad, Narasimha S.; Flood, Michael A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Campbell, JF (reprint author), NASA, Langley Res Ctr, 5 N Dryden St, Hampton, VA 23681 USA.
EM joel.f.campbell@nasa.gov
NR 10
TC 8
Z9 8
U1 0
U2 2
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
J9 OPT ENG
JI Opt. Eng.
PD DEC
PY 2011
VL 50
IS 12
AR 126002
DI 10.1117/1.3658758
PG 8
WC Optics
SC Optics
GA 865CX
UT WOS:000298289500034
ER
PT J
AU Kar, A
Stroscio, MA
Dutta, M
Meyyappan, M
AF Kar, Ayan
Stroscio, Michael A.
Dutta, Mitra
Meyyappan, M.
TI Electronic properties of Y-junctions in SnO2 nanowires
SO PHYSICA STATUS SOLIDI B-BASIC SOLID STATE PHYSICS
LA English
DT Article
DE nanowires; SnO2; vapor-liquid-solid mechanism; structure; photo-emission
spectroscopy
ID GROWTH; KINKING
AB Growth conditions leading to kinking and branching in SnO2 nanowires have been investigated. Lower temperature growth at 750 degrees C leads to Y-junctions as seen previously in carbon nanotubes, whereas straight nanowires are obtained at 880 degrees C. Photoemission valence band spectroscopy is used to show that the carrier concentration and Fermi level position vary with diameter. Thus, the stem and branches in a Y-junction can have completely different semiconducting properties, leading to opportunities in novel device construction. (C) 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim
C1 [Kar, Ayan; Stroscio, Michael A.; Dutta, Mitra] Univ Illinois, Dept Elect & Comp Engn, Chicago, IL 60607 USA.
[Stroscio, Michael A.; Dutta, Mitra] Univ Illinois, Dept Phys, Chicago, IL 60607 USA.
[Stroscio, Michael A.] Univ Illinois, Dept Bioengn, Chicago, IL 60607 USA.
[Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Kar, A (reprint author), Univ Illinois, Dept Elect & Comp Engn, Chicago, IL 60607 USA.
EM akar2@uic.edu
NR 27
TC 3
Z9 3
U1 1
U2 4
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0370-1972
J9 PHYS STATUS SOLIDI B
JI Phys. Status Solidi B-Basic Solid State Phys.
PD DEC
PY 2011
VL 248
IS 12
BP 2848
EP 2852
DI 10.1002/pssb.201147233
PG 5
WC Physics, Condensed Matter
SC Physics
GA 864TQ
UT WOS:000298263400013
ER
PT J
AU Perry, ME
Kahan, DS
Barnouin, OS
Ernst, CM
Solomon, SC
Zuber, MT
Smith, DE
Phillips, RJ
Srinivasan, DK
Oberst, J
Asmar, SW
AF Perry, Mark E.
Kahan, Daniel S.
Barnouin, Olivier S.
Ernst, Carolyn M.
Solomon, Sean C.
Zuber, Maria T.
Smith, David E.
Phillips, Roger J.
Srinivasan, Dipak K.
Oberst, Juergen
Asmar, Sami W.
TI Measurement of the radius of Mercury by radio occultation during the
MESSENGER flybys
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; MESSENGER; Occultation; RF; Radius
ID MISSION; SHAPE; SPACECRAFT; ALTIMETRY
AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft completed three flybys of Mercury in 2008-2009. During the first and third of those flybys. MESSENGER passed behind the planet from the perspective of Earth, occulting the radio-frequency (RF) transmissions. The occultation start and end times, recovered with 0.1 s accuracy or better by fitting edge-diffraction patterns to the RF power history, are used to estimate Mercury's radius at the tangent point of the RF path. To relate the measured radius to the planet shape, we evaluate local topography using images to identify the high-elevation feature that defines the RF path or using altimeter data to quantify surface roughness. Radius measurements are accurate to 150 m, and uncertainty in the average radius of the surrounding terrain, after adjustments are made from the local high at the tangent point of the RF path, is 350 m. The results are consistent with Mercury's equatorial shape as inferred from observations by the Mercury Laser Altimeter and ground-based radar. The three independent estimates of radius from occultation events collectively yield a mean radius for Mercury of 2439.2 +/- 0.5 km. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Perry, Mark E.; Barnouin, Olivier S.; Ernst, Carolyn M.; Srinivasan, Dipak K.] Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 21044 USA.
[Kahan, Daniel S.; Asmar, Sami W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA.
[Oberst, Juergen] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany.
RP Perry, ME (reprint author), Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 21044 USA.
EM mark.perry@jhuapl.edu
RI Ernst, Carolyn/I-4902-2012; Barnouin, Olivier/I-7475-2015; Perry,
Mark/B-8870-2016
OI Barnouin, Olivier/0000-0002-3578-7750; Perry, Mark/0000-0003-1600-6856
FU NASA [NAS5-97271, NASW-00002]
FX Details on the mission, flybys, and Mercury orbit insertion are
maintained and updated at the MESSENGER web site:
http://messenger.jhuapl.edu/. The MESSENGER mission is supported by the
NASA Discovery Program under contracts NAS5-97271 to the Johns Hopkins
University Applied Physics Laboratory and NASW-00002 to the Carnegie
Institution of Washington.
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 1925
EP 1931
DI 10.1016/j.pss.2011.07.022
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800010
ER
PT J
AU Sarantos, M
Killen, RM
McClintock, WE
Bradley, ET
Vervack, RJ
Benna, M
Slavin, JA
AF Sarantos, Menelaos
Killen, Rosemary M.
McClintock, William E.
Bradley, E. Todd
Vervack, Ronald J., Jr.
Benna, Mehdi
Slavin, James A.
TI Limits to Mercury's magnesium exosphere from MESSENGER second flyby
observations
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Mercury atmosphere; Mercury surface; Atmospheric structure;
Mercury magnetosphere; MESSENGER
ID SODIUM; MODEL; IMPACT; MAGNETOSPHERE; VAPORIZATION; ATMOSPHERE; LUNAR;
NAO
AB The discovery measurements of Mercury's exospheric magnesium, obtained by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) probe during its second Mercury flyby, are modeled to constrain the source and loss processes for this neutral species. Fits to a Chamberlain exosphere reveal that at least two source temperatures are required to reconcile the distribution of magnesium measured far from and near the planet: a hot ejection process at the equivalent temperature of several tens of thousands of degrees K, and a competing, cooler source at temperatures as low as 400 K. For the energetic component, our models indicate that the column abundance that can be attributed to sputtering under constant southward interplanetary magnetic field conditions is at least a factor of five less than the rate dictated by the measurements. Although highly uncertain, this result suggests that another energetic process, such as the rapid dissociation of exospheric MgO, may be the main source of the distant neutral component. If meteoroid and micrometeoroid impacts eject mainly molecules, the total amount of magnesium at altitudes exceeding similar to 100 km is found to be consistent with predictions by impact vaporization models for molecule lifetimes of no more than two minutes. Though a sharp increase in emission observed near the dawn terminator region can be reproduced if a single meteoroid enhanced the impact vapor at equatorial dawn, it is much more likely that observations in this region, which probe heights increasingly near the surface, indicate a reservoir of volatile Mg being acted upon by lower-energy source processes. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Sarantos, Menelaos; Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sarantos, Menelaos; Benna, Mehdi] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Killen, Rosemary M.] NASA, Planetary Magnetospheres Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McClintock, William E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Bradley, E. Todd] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Vervack, Ronald J., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Benna, Mehdi] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sarantos, M (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM menelaos.sarantos-1@nasa.gov
RI Benna, Mehdi/F-3489-2012; Slavin, James/H-3170-2012; Sarantos,
Menelaos/H-8136-2013; Vervack, Ronald/C-2702-2016
OI Slavin, James/0000-0002-9206-724X; Vervack, Ronald/0000-0002-8227-9564
FU NASA [NAS5-97271, NASW-00002]; MESSENGER
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to the Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington.
RMK, RJV, and MB are supported by the MESSENGER Participating Scientist
Program. MS thanks Apostolos Christou and Jeremie Vaubaillon for their
remarks on the possibility that a meteoroid stream affected Mercury
during the flyby observations, and Richard Hartle for his suggestions on
modeling exospheric dissociating ejecta.
NR 38
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 1992
EP 2003
DI 10.1016/j.pss.2011.05.002
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800016
ER
PT J
AU Raines, JM
Slavin, JA
Zurbuchen, TH
Gloeckler, G
Anderson, BJ
Baker, DN
Korth, H
Krimigis, SM
McNutt, RL
AF Raines, Jim M.
Slavin, James A.
Zurbuchen, Thomas H.
Gloeckler, George
Anderson, Brian J.
Baker, Daniel N.
Korth, Haje
Krimigis, Stamatios M.
McNutt, Ralph L., Jr.
TI MESSENGER observations of the plasma environment near Mercury
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Magnetosphere; Plasma; MESSENGER
ID 1ST FLYBY; MAGNETOSPHERE; SHEET; SPECTROMETER; INSTRUMENT; MISSION;
FLOWS; FIELD; MODEL; TAIL
AB The MESSENGER Fast Imaging Plasma Spectrometer (FIPS) measured the bulk plasma characteristics of Mercury's magnetosphere and solar wind environment during the spacecraft's first two flybys of the planet on 14 January 2008 (M1) and 6 October 2008 (M2), producing the first measurements of thermal ions in Mercury's magnetosphere. In this work, we identify major features of the Mercury magnetosphere in the FIPS proton data and describe the data analysis process used for recovery of proton density (n(p)) and temperature (T-p) with a forward modeling technique, required because of limitations in measurement geometry. We focus on three regions where the magnetospheric flow speed is likely to be low and meets our criteria for the recovery process: the M1 plasma sheet and the M1 and M2 dayside and nightside boundary-layer regions. Interplanetary magnetic field (IMF) conditions were substantially different between the two flybys, with intense reconnection signatures observed by the Magnetometer during M2 versus a relatively quiet magnetosphere during M1. The recovered ion density and temperature values for the M1 quiet-time plasma sheet yielded n(p)similar to 1-10 cm(-3), T-p similar to 2 x 10(6) K, and plasma beta similar to 2. The nightside boundary-layer proton densities during M1 and M2 were similar, at n(p)similar to 4-5 cm(-3), but the temperature during M1 (T-p similar to 4-8 x 10(6) K) was 50% less than during M2 (T-p similar to 8 x 106 K), presumably due to reconnection in the tail. The dayside boundary layer observed during M1 had a density of 16 cm-3 and temperature of 2 x 106 K, whereas during M2 this region was less dense and hotter (n(p)similar to 8 cm(-3) and T-p similar to 10 x 10(6) K), again, most likely due to magnetopause reconnection. Overall, the southward interplanetary magnetic field during M2 clearly produced higher T-p in the dayside and nightside magnetosphere, as well as higher plasma beta in the nightside boundary, similar to 20 during M2 compared with similar to 2 during M1. The proton plasma pressure accounts for only a fraction (24% for M1 and 64% for M2) of the drop in magnetic pressure upon entry into the dayside boundary layer. This result suggests that heavy ions of planetary origin, not considered in this analysis, may provide the "missing" pressure. If these planetary ions were hot due to "pickup" in the magnetosheath, the required density for pressure balance would be an ion density of similar to 1 cm(-3) for an ion temperature of similar to 10(8) K. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Raines, Jim M.; Zurbuchen, Thomas H.; Gloeckler, George] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, Brian J.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Krimigis, Stamatios M.] Acad Athens, Athens, Greece.
RP Raines, JM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA.
EM jraines@umich.edu; james.a.slavin@nasa.govm; thomasz@umich.edu;
gglo@umich.edu; Brian.Anderson@jhuapl.edu;
daniel.baker@lasp.colorado.edu; Haje.Korth@jhuapl.edu;
Tom.Krimigis@jhuapl.edu; Ralph.McNutt@jhuapl.edu
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166
FU MESSENGER; NASA [NAS5-97271, NASW-00002]
FX This work was funded by the MESSENGER project and a NASA Graduate
Student Research Program fellowship (JMR). The MESSENGER project is
supported by the NASA Discovery Program under contracts NAS5-97271 to
the Johns Hopkins University Applied Physics Laboratory and NASW-00002
to the Carnegie Institution of Washington. We acknowledge helpful
suggestions by Sean Solomon, MESSENGER Principal Investigator. JMR
gratefully acknowledges the help of Eli Busen, Aaron Dodger, and
Jonathon Thomas for their contributions to the FIPS software instrument
model and related software, and Deborah K. Eddy for help with manuscript
preparation. THZ acknowledges the hospitality of the International Space
Science Institute in Bern, Switzerland, where much of his contribution
to this work was performed.
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 2004
EP 2015
DI 10.1016/j.pss.2011.02.004
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800017
ER
PT J
AU Ho, GC
Starr, RD
Gold, RE
Krimigis, SM
Slavin, JA
Baker, DN
Anderson, BJ
McNutt, RL
Nittler, LR
Solomon, SC
AF Ho, George C.
Starr, Richard D.
Gold, Robert E.
Krimigis, Stamatios M.
Slavin, James A.
Baker, Daniel N.
Anderson, Brian J.
McNutt, Ralph L., Jr.
Nittler, Larry R.
Solomon, Sean C.
TI Observations of suprathermal electrons in Mercury's magnetosphere during
the three MESSENGER flybys
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Magnetosphere; Energetic particles; MESSENGER
ID X-RAY SPECTROMETER; ENERGETIC PARTICLE; MAGNETIC-FIELD; POPULATIONS;
INSTRUMENT; SPACECRAFT
AB In 2008 the MESSENGER spacecraft made the first direct observation of Mercury's magnetosphere in the more than 30 years since the Mariner 10 encounters. During MESSENGER's first flyby on 14 January 2008, the interplanetary magnetic field (IMF) was northward immediately prior to and following MESSENGER's equatorial passage through this small magnetosphere. The Energetic Particle Spectrometer (EPS), one of two sensors on the Energetic Particle and Plasma Spectrometer instrument that responds to electrons from similar to 35 key to 1 MeV and ions from similar to 35 key to 2.75 MeV, saw no increases in particle intensity above instrumental background (similar to 5 particles/cm(2)/sr/s/keV at 45 key) at any time during the probe's magnetospheric passage. During MESSENGER's second flyby on 6 October 2008, there was a steady southward IMF, and intense reconnection was observed between the planet's magnetic field and the IMF. However, once again EPS did not observe bursts of energetic particles similar to those reported by Mariner 10 from its March 1974 encounter. On 29 September 2009, MESSENGER flew by Mercury for the third and final time before orbit insertion in March 2011. Although a spacecraft safe-hold event stopped science measurements prior to the outbound portion of the flyby, all instruments recorded full observations until a few minutes before the closest approach. In particular, the MESSENGER Magnetometer documented several substorm-like signatures of extreme loading of Mercury's magnetotail, but again EPS measured no energetic ions or electrons above instrument background during the inbound portion of the flyby. MESSENGER's X-Ray Spectrometer (XRS) nonetheless observed photons resulting from low-energy (similar to 10 key) electrons impinging on its detectors during each of the three flybys. We infer that suprathermal plasma electrons below the EPS energy threshold caused the bremsstrahlung seen by XRS. In this paper, we summarize the energetic particle observations made by EPS and XRS during MESSENGER's three Mercury flybys, and we revisit the observations reported by Mariner 10 in the context of these new results. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Ho, George C.; Gold, Robert E.; Krimigis, Stamatios M.; Anderson, Brian J.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Krimigis, Stamatios M.] Acad Athens, Off Space Res & Technol, Athens 71527, Greece.
[Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Ho, GC (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM George.Ho@jhuapl.edu
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010; Ho, George/G-3650-2015
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166;
Ho, George/0000-0003-1093-2066
FU NASA through the NASA Center for Computational Sciences (NCCS) at the
Goddard Space Flight Center; NASA [NASW-00002, NAS5-97271]
FX The authors acknowledge the large number of scientists and engineers at
The Johns Hopkins University Applied Physics Laboratory who contributed
their technical expertise and skill to the successful development of the
EPS sensor. Resources supporting the XRS analysis were provided by the
NASA High-End Computing (HEC) Program through the NASA Center for
Computational Sciences (NCCS) at the Goddard Space Flight Center. The
MESSENGER project is supported by the NASA Discovery Program under
contracts NASW-00002 to the Carnegie Institution of Washington and
NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory.
NR 27
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 2016
EP 2025
DI 10.1016/j.pss.2011.01.011
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800018
ER
PT J
AU Schriver, D
Travnicek, P
Ashour-Abdalla, M
Richard, RL
Hellinger, P
Slavin, JA
Anderson, BJ
Baker, DN
Benna, M
Boardsen, SA
Gold, RE
Ho, GC
Korth, H
Krimigis, SM
McClintock, WE
McLain, JL
Orlando, TM
Sarantos, M
Sprague, AL
Starr, RD
AF Schriver, David
Travnicek, Pavel
Ashour-Abdalla, Maha
Richard, Robert L.
Hellinger, Petr
Slavin, James A.
Anderson, Brian J.
Baker, Daniel N.
Benna, Mehdi
Boardsen, Scott A.
Gold, Robert E.
Ho, George C.
Korth, Haje
Krimigis, Stamatios M.
McClintock, William E.
McLain, Jason L.
Orlando, Thomas M.
Sarantos, Menelaos
Sprague, Ann L.
Starr, Richard D.
TI Electron transport and precipitation at Mercury during the MESSENGER
flybys: Implications for electron-stimulated desorption
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Magnetosphere; Numerical simulations; Electron transport;
Electron-stimulated desorption; MESSENGER
ID SOLAR-WIND INTERACTION; 3-DIMENSIONAL HYBRID SIMULATION; MAGNETIC-FIELD;
PLASMA SHEET; MAGNETOTAIL RECONNECTION; UNMAGNETIZED PLANETS; SODIUM
EXOSPHERE; FORCE BALANCE; ION DYNAMICS; 1ST FLYBY
AB To examine electron transport, energization, and precipitation in Mercury's magnetosphere, a hybrid simulation study has been carried out that follows electron trajectories within the global magnetospheric electric and magnetic field configuration of Mercury. We report analysis for two solar-wind parameter conditions corresponding to the first two MESSENGER Mercury flybys on January 14, 2008, and October 6, 2008, which occurred for similar solar wind speed and density but contrasting interplanetary magnetic field (IMF) directions. During the first flyby the IMF had a northward component, while during the second flyby the IMF was southward. Electron trajectories are traced in the fields of global hybrid simulations for the two flybys. Some solar wind electrons follow complex trajectories at or near where dayside reconnection occurs and enter the magnetosphere at these locations. The entry locations depend on the IMF orientation (north or south). As the electrons move through the entry regions they can be energized as they execute non-adiabatic (demagnetized) motion. Some electrons become magnetically trapped and drift around the planet with energies on the order of 1-10 key. The highest energy of electrons anywhere in the magnetosphere is about 25 key, consistent with the absence of high-energy (> 35 key) electrons observed during either MESSENGER flyby. Once within the magnetosphere, a fraction of the electrons precipitates at the planetary surface with fluxes on the order of 10(9) cm(-2) s(-1) and with energies of hundreds of eV. This finding has important implications for the viability of electron-stimulated desorption (ESD) as a mechanism for contributing to the formation of the exosphere and heavy ion cloud around Mercury. From laboratory estimates of ESD ion yields, a calculated ion production rate due to ESD at Mercury is found to be on par with ion sputtering yields. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Schriver, David; Ashour-Abdalla, Maha; Richard, Robert L.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90025 USA.
[Ashour-Abdalla, Maha] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Travnicek, Pavel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Travnicek, Pavel; Hellinger, Petr] ASCR, Astron Inst, Prague 14131, Czech Republic.
[Slavin, James A.; Boardsen, Scott A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, Brian J.; Gold, Robert E.; Ho, George C.; Korth, Haje; Krimigis, Stamatios M.; Sarantos, Menelaos] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Baker, Daniel N.; McClintock, William E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Benna, Mehdi] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimigis, Stamatios M.] Acad Athens, Off Space Res Technol, Athens 11527, Greece.
[McLain, Jason L.; Orlando, Thomas M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA.
[McLain, Jason L.; Orlando, Thomas M.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Schriver, D (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90025 USA.
EM dave@igpp.ucla.edu
RI Benna, Mehdi/F-3489-2012; Anderson, Brian/I-8615-2012; Slavin,
James/H-3170-2012; Sarantos, Menelaos/H-8136-2013; Hellinger,
Petr/F-5267-2014; Travnicek, Pavel/G-8608-2014; Ho, George/G-3650-2015
OI Slavin, James/0000-0002-9206-724X; Hellinger, Petr/0000-0002-5608-0834;
Ho, George/0000-0003-1093-2066
FU NASA MESSENGER [NNX07AR62G, NNX07AV79G, NNX09AD41G]; NASA [NNX09AJ73G,
NNG06-GG20G]; Czech Ministry of Education [ME09009]; European Space
Agency [98068]
FX This work was supported by NASA MESSENGER grants NNX07AR62G, NNX07AV79G,
and NNX09AD41G, NASA LWS Grant NNX09AJ73G, NASA Planetary Atmospheres
Program NNG06-GG20G, contract ME09009 of the Czech Ministry of
Education, and PECS contract 98068 from the European Space Agency.
Computing was carried out on the NASA Advanced Supercomputing (NAS)
Silicon Graphics Altix machine as part of the Columbia supercomputing
system and the National Science Foundation (NSF) National Center for
Atmospheric Research (NCAR) Frost Blue Gene supercomputing system.
Global hybrid simulations used for this work were performed on the
Amalka supercomputing facility at the Institute of Atmospheric Physics,
Academy of Sciences of the Czech Republic.
NR 97
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 2026
EP 2036
DI 10.1016/j.pss.2011.03.008
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800019
ER
PT J
AU Anderson, BJ
Slavin, JA
Korth, H
Boardsen, SA
Zurbuchen, TH
Raines, JM
Gloeckler, G
McNutt, RL
Solomon, SC
AF Anderson, Brian J.
Slavin, James A.
Korth, Haje
Boardsen, Scott A.
Zurbuchen, Thomas H.
Raines, Jim M.
Gloeckler, George
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI The dayside magnetospheric boundary layer at Mercury
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Magnetosphere; Boundary layer; Magnetic field; Plasma;
MESSENGER
ID FIELD-ALIGNED CURRENTS; MESSENGERS 1ST FLYBY; MAGNETIC-FIELD; EXOSPHERE;
INSTRUMENT; PARTICLE; PROTON
AB Magnetic field and plasma data from the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft on the outbound portions of the first (M1) and second (M2) flybys of Mercury reveal a region of depressed magnetic field magnitude and enhanced proton fluxes adjacent to but within the magnetopause, which we denote as a dayside boundary layer. The layer was present during both encounters despite the contrasting dayside magnetic reconnection, which was minimal during M1 and strong during M2. The overall width of the layer is estimated to be between 1000 and 1400 km, spanning most of the distance from the dayside planetary surface to the magnetopause in the mid-morning. During both flybys the magnetic pressure decrease was similar to 1.6 nPa, and the width of the inner edge was comparable to proton gyro-kinetic scales. The maximum variance in the magnetic field across the inner edge was aligned with the magnetic field vector, and the magnetic field direction did not change markedly, indicating that the change in field intensity was consistent with an outward plasma-pressure gradient perpendicular to the magnetic field. Proton pressures in the layer inferred from reduced distribution observations were 0.4 nPa during M1 and 1.0 nPa during M2, indicating either that the proton pressure estimates are low or that heavy ions contribute substantially to the boundary-layer plasma pressure. If the layer is formed by protons drifting westward from the cusp, there should be a strong morning-afternoon asymmetry that is independent of the interplanetary magnetic field (IMF) direction. Conversely, if heavy ions play a major role, the layer should be strong in the morning (afternoon) for northward (southward) IMF. Future MESSENGER observations from orbit about Mercury should distinguish between these two possibilities. (C) 2011 Published by Elsevier Ltd.
C1 [Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Slavin, James A.; Boardsen, Scott A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Zurbuchen, Thomas H.; Raines, Jim M.; Gloeckler, George] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Anderson, BJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM brian.anderson@jhuapl.edu
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166
FU NASA [NASW-00002, NAS5-97271]
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NASW-00002 to the Carnegie Institution of Washington and
NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory.
NR 38
TC 15
Z9 15
U1 0
U2 5
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 DEC
PY 2011
VL 59
IS 15
SI SI
BP 2037
EP 2050
DI 10.1016/j.pss.2011.01.010
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800020
ER
PT J
AU Sundberg, T
Boardsen, SA
Slavin, JA
Blomberg, LG
Cumnock, JA
Solomon, SC
Anderson, BJ
Korth, H
AF Sundberg, Torbjorn
Boardsen, Scott A.
Slavin, James A.
Blomberg, Lars G.
Cumnock, Judy A.
Solomon, Sean C.
Anderson, Brian J.
Korth, Haje
TI Reconstruction of propagating Kelvin-Helmholtz vortices at Mercury's
magnetopause
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Kelvin-Helmholtz; Magnetopause; MESSENGER
ID INTERPLANETARY MAGNETIC-FIELD; SOLAR-WIND; MAGNETOSPHERIC BOUNDARY;
MESSENGER OBSERVATIONS; MAGNETOTAIL BOUNDARY; CLUSTER OBSERVATIONS;
GEOTAIL OBSERVATIONS; PLASMA ENVIRONMENT; SURFACE-WAVES; INSTABILITY
AB A series of quasi-periodic magnetopause crossings were recorded by the MESSENGER spacecraft during its third flyby of Mercury on 29 September 2009, likely caused by a train of propagating Kelvin-Helmholtz (KH) vortices. We here revisit the observations to study the internal structure of the waves. Exploiting MESSENGER's rapid traversal of the magnetopause, we show that the observations permit a reconstruction of the structure of a rolled-up KH vortex directly from the spacecraft's magnetic field measurements. The derived geometry is consistent with all large-scale fluctuations in the magnetic field data, establishes the non-linear nature of the waves, and shows their vortex-like structure. In several of the wave passages, a reduction in magnetic field strength is observed in the middle of the wave, which is characteristic of rolled-up vortices and is related to the increase in magnetic pressure required to balance the centrifugal force on the plasma in the outer regions of a vortex, previously reported in computer simulations. As the KH wave starts to roll up, the reconstructed geometry suggests that the vortices develop two gradual transition regions in the magnetic field, possibly related to the mixing of magnetosheath and magnetospheric plasma, situated at the leading edges from the perspectives of both the magnetosphere and the magnetosheath. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Sundberg, Torbjorn; Blomberg, Lars G.; Cumnock, Judy A.] Royal Inst Technol KTH, Sch Elect Engn, Stockholm, Sweden.
[Boardsen, Scott A.; Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Cumnock, Judy A.] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75083 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Sundberg, T (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM torbjorn.sundberg@nasa.gov
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU Swedish National Space Board; NASA [NASW-00002, NAS5-97271]
FX This work was partially supported by the Swedish National Space Board.
The MESSENGER project is supported by the NASA Discovery Program under
contracts NASW-00002 to the Carnegie Institution of Washington and
NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory.
NR 42
TC 14
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U1 2
U2 10
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 DEC
PY 2011
VL 59
IS 15
SI SI
BP 2051
EP 2057
DI 10.1016/j.pss.2011.05.008
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800021
ER
PT J
AU Milan, SE
Slavin, JA
AF Milan, S. E.
Slavin, J. A.
TI An assessment of the length and variability of Mercury's magnetotail
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Magnetosphere; Magnetotail; Substorm; Solar wind-magnetosphere
coupling
ID INTERPLANETARY MAGNETIC-FIELD; MESSENGER OBSERVATIONS; FLUX-TRANSFER;
SOLAR-WIND; MAGNETOSPHERE; RECONNECTION; OBJECTIVES; DYNAMICS; ROTATION;
MISSION
AB We employ Mariner 10 measurements of the interplanetary magnetic field in the vicinity of Mercury to estimate the rate of magnetic reconnection between the interplanetary magnetic field and the Hermean magnetosphere. We derive a time-series of the open magnetic flux in Mercury's magnetosphere, from which we can deduce the length of the magnetotail. The length of the magnetotail is shown to be highly variable, with open field lines stretching between 15R(H) and 850R(H) downstream of the planet (median 150R(H)). Scaling laws allow the tail length at perihelion to be deduced from the aphelion Mariner 10 observations. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Milan, S. E.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Slavin, J. A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Milan, SE (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM steve.milan@ion.le.ac.uk
RI Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU STFC [PP/E000983/1]
FX SEM was supported by STFC grant STFC rolling Grant no. PP/E000983/1.
NR 38
TC 5
Z9 5
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 2058
EP 2065
DI 10.1016/j.pss.2011.05.007
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800022
ER
PT J
AU Baker, DN
Odstrcil, D
Anderson, BJ
Arge, CN
Benna, M
Gloeckler, G
Korth, H
Mayer, LR
Raines, JM
Schriver, D
Slavin, JA
Solomon, SC
Travnicek, PM
Zurbuchen, TH
AF Baker, Daniel N.
Odstrcil, Dusan
Anderson, Brian J.
Arge, C. Nick
Benna, Mehdi
Gloeckler, George
Korth, Haje
Mayer, Leslie R.
Raines, Jim M.
Schriver, David
Slavin, James A.
Solomon, Sean C.
Travnicek, Pavel M.
Zurbuchen, Thomas H.
TI The space environment of Mercury at the times of the second and third
MESSENGER flybys
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Solar wind; Interplanetary magnetic field; Magnetospheres;
MESSENGER
ID MAGNETIC-FIELD; SOLAR-WIND; 1ST FLYBY; MAGNETOSPHERE; MODEL
AB The second and third flybys of Mercury by the MESSENGER spacecraft occurred, respectively, on 6 October 2008 and on 29 September 2009. In order to provide contextual information about the solar wind properties and the interplanetary magnetic field (IMF) near the planet at those times, we have used an empirical modeling technique combined with a numerical physics-based solar wind model. The Wang-Sheeley-Arge (WSA) method uses solar photospheric magnetic field observations (from Earth-based instruments) in order to estimate the inner heliospheric radial flow speed and radial magnetic field out to 21.5 solar radii from the Sun. This information is then used as input to the global numerical magnetohydrodynamic model, ENLIL, which calculates solar wind velocity, density, temperature, and magnetic field strength and polarity throughout the inner heliosphere. WSA-ENLIL calculations are presented for the several-week period encompassing the second and third flybys. This information, in conjunction with available MESSENGER data, aid in understanding the Mercury flyby observations and provide a basis for global magnetospheric modeling. We find that during both flybys, the solar wind conditions were very quiescent and would have provided only modest dynamic driving forces for Mercury's magnetospheric system. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Odstrcil, Dusan] George Mason Univ, Fairfax, VA 22030 USA.
[Odstrcil, Dusan; Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Arge, C. Nick] USAF, Res Lab, Kirtland AFB, NM 87117 USA.
[Benna, Mehdi] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gloeckler, George; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Mayer, Leslie R.] NOAA, Boulder, CO 80303 USA.
[Schriver, David; Travnicek, Pavel M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Travnicek, Pavel M.] ASCR, Astron Inst, Prague 14131, Czech Republic.
[Travnicek, Pavel M.] ASCR, Inst Atmospher Phys, Prague 14131, Czech Republic.
RP Baker, DN (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
EM daniel.baker@lasp.colorado.edu
RI Benna, Mehdi/F-3489-2012; Anderson, Brian/I-8615-2012; Slavin,
James/H-3170-2012; Travnicek, Pavel/G-8608-2014
OI Slavin, James/0000-0002-9206-724X;
FU NASA [NASW-00002, NAS5-97271]; National Science Foundation's Center for
Integrated Space Weather Modeling
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NASW-00002 to the Carnegie Institution of Washington and
NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory.
The modeling techniques described here were originally developed under
the auspices of the National Science Foundation's Center for Integrated
Space Weather Modeling.
NR 21
TC 17
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U1 0
U2 2
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 DEC
PY 2011
VL 59
IS 15
SI SI
BP 2066
EP 2074
DI 10.1016/j.pss.2011.01.018
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800023
ER
PT J
AU Korth, H
Anderson, BJ
Zurbuchen, TH
Slavin, JA
Perri, S
Boardsen, SA
Baker, DN
Solomon, SC
McNutt, RL
AF Korth, Haje
Anderson, Brian J.
Zurbuchen, Thomas H.
Slavin, James A.
Perri, Silvia
Boardsen, Scott A.
Baker, Daniel N.
Solomon, Sean C.
McNutt, Ralph L., Jr.
TI The interplanetary magnetic field environment at Mercury's orbit
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Interplanetary magnetic field; Inner heliosphere; Mercury; MESSENGER
ID SOLAR-WIND; DISSIPATION RANGE; POWER SPECTRA; FLUCTUATIONS; TURBULENCE;
HELIOS-1; MESSENGER; AU; DEPENDENCE; SPACECRAFT
AB Mercury is exposed to the most dynamic heliospheric space environment of any planet in the solar system. The magnetosphere is particularly sensitive to variations in the interplanetary magnetic field (IMF), which control the intensity and geometry of the magnetospheric current systems that are the dominant source of uncertainty in determinations of the internal planetary magnetic field structure. The Magnetometer on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft has made extensive magnetic field observations in the inner heliosphere over the heliocentric distances of Mercury's orbit, between 0.31 and 0.47 AU. In this paper, Magnetometer data from MESSENGER, obtained at rates of 2 and 20 vector samples per second, are used together with previous observations in the inner heliosphere by Helios and at Earth by the Advanced Composition Explorer, to study the characteristics of IMF variability at Mercury's orbit. Although the average IMF geometry and magnitude depend on heliocentric distance as predicted by Parker, the variability is large, comparable to the total field magnitude. Using models for the external current systems we evaluate the impact of the variability on the field near the planet and find that the large IMF fluctuations should produce variations of the magnetospheric field of up to 30% of the dipole field at 200 km altitude, corresponding to the planned periapsis of MESSENGER's orbit at Mercury. The IMF fluctuations in the frequency range 10(-4) < f < 10(-1) Hz are consistent with turbulence, whereas evidence for dissipation was observed for f > 1 Hz. The transition between the turbulent and dissipative regimes is indicated by a break in the power spectrum, and the frequency of this break point is proportional to the IMF magnitude. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Korth, Haje; Anderson, Brian J.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Slavin, James A.; Boardsen, Scott A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Perri, Silvia] Int Space Sci Inst, Bern, Switzerland.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Korth, H (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM haje.korth@jhuapl.edu
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166
FU NASA [NASW-00002, NAS5-97271]
FX We thank the ACE team for use of magnetometer data made available via
the ACE Level 2 database, and the National Space Science Data Center
(NSSDC) for supplying the Helios data set. T.H.Z. acknowledges the
hospitality of the International Space Science Institute where most of
his work was performed. The MESSENGER project is supported by the NASA
Discovery Program under contracts NASW-00002 to the Carnegie Institution
of Washington and NAS5-97271 to the Johns Hopkins University Applied
Physics Laboratory.
NR 57
TC 14
Z9 14
U1 0
U2 3
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 DEC
PY 2011
VL 59
IS 15
SI SI
BP 2075
EP 2085
DI 10.1016/j.pss.2010.10.014
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800024
ER
PT J
AU Ray, RD
Douglas, BC
AF Ray, Richard D.
Douglas, Bruce C.
TI Experiments in reconstructing twentieth-century sea levels
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Review
ID TIDE-GAUGE DATA; DATA ASSIMILATION; SURFACE; OCEAN; RISE;
TOPEX/POSEIDON; FREQUENCY; CIRCULATION; GREENLAND; JASON-1
AB One approach to reconstructing historical sea level from the relatively sparse tide-gauge network is to employ Empirical Orthogonal Functions (EOFs) as interpolatory spatial basis functions. The EOFs are determined from independent global data, generally sea-surface heights from either satellite altimetry or a numerical ocean model. The problem is revisited here for sea level since 1900. A new approach to handling the tide-gauge datum problem by direct solution offers possible advantages over the method of integrating sea-level differences, with the potential of eventually adjusting datums into the global terrestrial reference frame. The resulting time series of global mean sea levels appears fairly insensitive to the adopted set of EOFs. In contrast, charts of regional sea level anomalies and trends are very sensitive to the adopted set of EOFs, especially for the sparser network of gauges in the early 20th century. The reconstructions appear especially suspect before 1950 in the tropical Pacific. While this limits some applications of the sea-level reconstructions, the sensitivity does appear adequately captured by formal uncertainties. All our solutions show regional trends over the past five decades to be fairly uniform throughout the global ocean, in contrast to trends observed over the shorter altimeter era. Consistent with several previous estimates, the global sea-level rise since 1900 is 1.70 +/- 0.26 mm yr(-1). The global trend since 1995 exceeds 3 mm yr(-1) which is consistent with altimeter measurements, but this large trend was possibly also reached between 1935 and 1950. Published by Elsevier Ltd.
C1 [Ray, Richard D.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Douglas, Bruce C.] Florida Int Univ, Miami, FL 33199 USA.
RP Ray, RD (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM richard.ray@nasa.gov
RI Ray, Richard/D-1034-2012
FU US National Aeronautics and Space Administration under the IDS
FX Work of this kind owes immeasurably to generations of anonymous
tide-gauge operators as well as to the Permanent Service for Mean Sea
Level, which has benefited our work and nearly all similar studies of
historic sea levels. Brian Beckley provided essential help with handling
the satellite altimeter data. Anthony Weaver and Philippe Rogel kindly
provided the outputs from the OPA/NEMO ocean model. For fruitful
discussions we thank Mark Merrifield, Laury Miller, and Philip
Woodworth. This work was supported by the US National Aeronautics and
Space Administration under the IDS Sea Level program.
NR 70
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U1 2
U2 30
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0079-6611
J9 PROG OCEANOGR
JI Prog. Oceanogr.
PD DEC
PY 2011
VL 91
IS 4
BP 496
EP 515
DI 10.1016/j.pocean.2011.07.021
PG 20
WC Oceanography
SC Oceanography
GA 863XQ
UT WOS:000298202000010
ER
PT J
AU O'Connor, DP
Mahar, MT
Laughlin, MS
Jackson, AS
AF O'Connor, Daniel P.
Mahar, Matthew T.
Laughlin, Mitzi S.
Jackson, Andrew S.
TI The Bland-Altman Method Should Not Be Used in Regression
Cross-Validation Studies
SO RESEARCH QUARTERLY FOR EXERCISE AND SPORT
LA English
DT Article
DE bias; calibration; difference plots; measurement error
ID RESTING ENERGY-EXPENDITURE; PREDICTING BODY DENSITY; GENERALIZED
EQUATIONS; SPORTS-MEDICINE; STATISTICAL-METHODS; AGREEMENT; CHILDREN;
RELIABILITY; ADOLESCENTS; VARIABLES
AB The purpose of this study was to demonstrate the bias in the Bland-Altman (BA) limits of agreement method when it is used to validate regression models. Data from 1,158 men were used to develop three regression equations to estimate maximum oxygen uptake (R-2 = .40, .61, and .82, respectively). The equations were evaluated in a cross-validation sample of 581 men. The BA means and differences were correlated (p < .001) in the cross-validation sample for each model (r = .55, .39, and .26, respectively), thus demonstrating bias. The BA method is inappropriate for validation of regression models. Validation of regression equations is properly conducted by plotting the residuals against the estimated values and examining the magnitude of the estimation error
C1 [O'Connor, Daniel P.; Jackson, Andrew S.] Univ Houston, Dept Hlth & Human Performance, Houston, TX 77204 USA.
[Mahar, Matthew T.] E Carolina Univ, Dept Exercise & Sport Sci, Greenville, NC 27858 USA.
[Laughlin, Mitzi S.] NASA, Johnson Space Ctr, Houston, TX USA.
RP O'Connor, DP (reprint author), Univ Houston, Dept Hlth & Human Performance, 3855 Holman GAR104, Houston, TX 77204 USA.
EM doconnor2@uh.edu
NR 37
TC 6
Z9 6
U1 1
U2 9
PU AMER ALLIANCE HEALTH PHYS EDUC REC & DANCE
PI RESTON
PA 1900 ASSOCIATION DRIVE, RESTON, VA 22091 USA
SN 0270-1367
J9 RES Q EXERCISE SPORT
JI Res. Q. Exerc. Sport
PD DEC
PY 2011
VL 82
IS 4
BP 610
EP 616
PG 7
WC Hospitality, Leisure, Sport & Tourism; Psychology, Applied; Psychology;
Sport Sciences
SC Social Sciences - Other Topics; Psychology; Sport Sciences
GA 859MR
UT WOS:000297881000003
PM 22276402
ER
PT J
AU Landau, D
Strange, NJ
AF Landau, Damon
Strange, Nathan J.
TI More Than One Way to Reach into Space
SO SCIENTIFIC AMERICAN
LA English
DT Article
C1 [Landau, Damon] NASA, JPL, Washington, DC 20546 USA.
RP Landau, D (reprint author), NASA, JPL, Washington, DC 20546 USA.
NR 0
TC 1
Z9 1
U1 0
U2 2
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 0036-8733
J9 SCI AM
JI Sci.Am.
PD DEC
PY 2011
VL 305
IS 6
BP 60
EP 65
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 873EJ
UT WOS:000298863500029
ER
PT J
AU Tao, WK
Shi, JJ
Lin, PL
Chen, J
Lang, S
Chang, MY
Yang, MJ
Wu, CC
Peters-Lidard, C
Sui, CH
Jou, BJD
AF Tao, Wei-Kuo
Shi, Jainn Jong
Lin, Pay-Lin
Chen, Jhihying
Lang, Stephen
Chang, Mei-Yu
Yang, Ming-Jen
Wu, Chun-Chien
Peters-Lidard, Christa
Sui, Chung-Hsiung
Jou, Ben Jong-Dao
TI High-Resolution Numerical Simulation of the Extreme Rainfall Associated
with Typhoon Morakot. Part I: Comparing the Impact of Microphysics and
PBL Parameterizations with Observations
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Article; Proceedings Paper
CT International Workshop on Typhoon Morakot
CY MAR 25-26, 2010
CL Natl Taiwan Univ, Taipei, PEOPLES R CHINA
HO Natl Taiwan Univ
DE Typhoon Morakot; Cloud resolution model
ID PLANETARY BOUNDARY-LAYER; CLOUD MODEL; TROPICAL CYCLONES; BULK
PARAMETERIZATION; MICROSCALE STRUCTURE; CONVECTIVE SYSTEMS; VERTICAL
DIFFUSION; FRONTAL RAINBANDS; SITU OBSERVATIONS; HEAVY RAINFALL
AB Typhoon Morakot hit Taiwan the night of 7 August 2009 as a Category 1 storm and caused up to 3000 mm of rain, leading to the worst flooding there in 50 years as well as devastating mudslides. The Weather Research and Forecasting model (WRF) is used at high resolution to simulate this extreme weather event. The model results indicate that WRF is able to capture the amount and location of the observed surface rainfall and that the typhoon-induced circulation, orographic lifting and a moisture-abundant southwest flow are the main mechanisms that together produced the tremendous rainfall in this case. Furthermore, the model results suggest that the agreement with the observed rainfall is due to the simulated storm track and intensity being in relatively good agreement with the observed. Additional simulations were made to examine the sensitivity of this case to model physics (microphysics and planetary boundary layer or PBL). Both warm rain only as well as improved microphysics yield similar significant rain amounts at the same locations as the control case. The improved microphysics lead to a better storm intensity early on but later exceed the observed intensities by about 10 hPa. The stronger storm arises from less evaporative cooling from cloud and rain and consequently weaker simulated downdrafts. Warm rain results closely match the control (i.e., the track, intensity, and maximum rainfall locations/amounts), implying ice processes (i.e., additional heat release due to ice processes) have only a secondary effect on surface rainfall. Results are less sensitive to using different PBL schemes than different microphysics.
C1 [Tao, Wei-Kuo; Shi, Jainn Jong; Lang, Stephen] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Shi, Jainn Jong] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Lin, Pay-Lin; Chen, Jhihying; Yang, Ming-Jen] Natl Cent Univ, Dept Atmospher Sci, Jhongli, Taiwan.
[Lang, Stephen] Sci Syst & Applicat Inc, Lanham, MD USA.
[Chang, Mei-Yu] Cent Weather Bur, Taipei, Taiwan.
[Wu, Chun-Chien; Sui, Chung-Hsiung; Jou, Ben Jong-Dao] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan.
[Peters-Lidard, Christa] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Tao, WK (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
EM wei-kuo.tao-1@nasa.gov
RI Peters-Lidard, Christa/E-1429-2012; Yang, Ming-Jen/F-4628-2012;
OI Peters-Lidard, Christa/0000-0003-1255-2876; Yang,
Ming-Jen/0000-0001-6654-2791; JOU, BEN JONG DAO/0000-0001-5715-042X;
SUI, CHUNG-HSIUNG/0000-0003-2842-5660
NR 68
TC 23
Z9 26
U1 3
U2 19
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD DEC
PY 2011
VL 22
IS 6
SI SI
BP 673
EP 696
DI 10.3319/TAO.2011.08.26.01(TM)
PG 24
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA 873GF
UT WOS:000298868400011
ER
PT J
AU Case, JL
Kumar, SV
Srikishen, J
Jedlovec, GJ
AF Case, Jonathan L.
Kumar, Sujay V.
Srikishen, Jayanthi
Jedlovec, Gary J.
TI Improving Numerical Weather Predictions of Summertime Precipitation over
the Southeastern United States through a High-Resolution Initialization
of the Surface State
SO WEATHER AND FORECASTING
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; LAND-COVER DATA; SOIL-MOISTURE; ETA-MODEL;
WARM-SEASON; PART I; CONVECTION INITIATION; VEGETATION FRACTION;
BOUNDARY-LAYER; REAL-TIME
AB It is hypothesized that high-resolution. accurate representations of surface properties such as soil moisture and sea surface temperature are necessary to improve simulations of summertime pulse-type convective precipitation in high-resolution models. This paper presents model verification results of a case study period from June to August 2008 over the southeastern United States using the Weather Research and Forecasting numerical weather prediction model. Experimental simulations initialized with high-resolution land surface fields from the National Aeronautics and Space Administration's (NASA) Land Information System (LIS) and sea surface temperatures (SSTs) derived from the Moderate Resolution Imaging Spectroradiometer (MOD'S) are compared to a set of control simulations initialized with interpolated fields from the National Centers for Environmental Prediction's (NCEP) 12-km North American Mesoscale model. The LIS land surface and MOD IS SSTs provide a more detailed surface initialization at a resolution comparable to the 4-km model grid spacing. Soil moisture from the LIS spinup run is shown to respond better to the extreme rainfall of Tropical Storm Fay in August 2008 over the Florida peninsula. The LIS has slightly lower errors and higher anomaly correlations in the top soil layer but exhibits a stronger dry bias in the root zone. The model sensitivity to the alternative surface initial conditions is examined for a sample case, showing that the LIS-MODIS data substantially impact surface and boundary layer properties. The Developmental Testbed Center's Meteorological Evaluation Tools package is employed to produce verification statistics, including traditional gridded precipitation verification and output statistics from the Method for Object-Based Diagnostic Evaluation (MODE) tool. The LIS-MODIS initialization is found to produce small improvements in the skill scores of 1-h accumulated precipitation during the forecast hours of the peak diurnal convective cycle. Because there is very little union in time and space between the forecast and observed precipitation systems, results from the MODE object verification are examined to relax the stringency of traditional gridpoint precipitation verification. The MODE results indicate that the LIS-MODIS-initialized model runs increase the 10 mm h(-1) matched object areas ("hits") while simultaneously decreasing the unmatched object areas ("misses" plus "false alarms") during most of the peak convective forecast hours, with statistically significant improvements of up to 5%. Simulated 1-h precipitation objects in the LIS-MODIS runs more closely resemble the observed objects, particularly at higher accumulation thresholds. Despite the small improvements, however, the overall low verification scores indicate that much uncertainty still exists in simulating the processes responsible for airmass-type convective precipitation systems in convection-allowing models.
C1 [Case, Jonathan L.] ENSCO Inc, Short Term Predict Res & Transit SPoRT Ctr, Huntsville, AL USA.
[Kumar, Sujay V.] NASA, Goddard Space Flight Ctr, SAIC, Greenbelt, MD 20771 USA.
[Srikishen, Jayanthi] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Jedlovec, Gary J.] NASA, George C Marshall Space Flight Ctr, SPoRT Ctr, Huntsville, AL 35812 USA.
RP Case, JL (reprint author), Natl Space Sci & Technol Ctr, Rm 3062,320 Sparkman Dr, Huntsville, AL 35805 USA.
EM jonathan.case-1@nasa.gov
RI Kumar, Sujay/B-8142-2015
FU NASA Science Mission Directorate's Earth Science Division at the NASA
MSFC
FX This research was funded by Dr. Tsengdar Lee of the NASA Science Mission
Directorate's Earth Science Division in support of the SPoRT program at
the NASA MSFC. Computational resources for this work were provided by
the NASA Center for Climate Simulation at the NASA Goddard Space Flight
Center. The lead author is indebted to the invaluable assistance
provided by John Halley-Gotway and others on the MET development team at
NCAR. The authors also greatly appreciate the valuable contributions by
three anonymous reviewers and Dr. Joseph Santanello of the Goddard Space
Flight Center. Mention of a copyrighted, trademarked, or proprietary
product, service, or document does not constitute endorsement thereof by
the authors, ENSCO Inc., SAIC, USRA, the SPoRT Center, the National
Aeronautics and Space Administration, or the U.S. government. Any such
mention is solely for the purpose of fully informing the reader of the
resources used to conduct the work reported herein.
NR 63
TC 22
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U1 0
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
J9 WEATHER FORECAST
JI Weather Forecast.
PD DEC
PY 2011
VL 26
IS 6
BP 785
EP 807
DI 10.1175/2011WAF2222455.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 864UC
UT WOS:000298264600001
ER
PT J
AU Reale, O
Lau, KM
da Silva, A
AF Reale, Oreste
Lau, K. M.
da Silva, Arlindo
TI Impact of Interactive Aerosol on the African Easterly Jet in the NASA
GEOS-5 Global Forecasting System (vol 26, pg 504, 2011)
SO WEATHER AND FORECASTING
LA English
DT Correction
C1 [Reale, Oreste; Lau, K. M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[da Silva, Arlindo] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Reale, Oreste] Univ Space Res Assoc, Columbia, MD USA.
RP Reale, O (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
EM oreste.reale-1@nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
J9 WEATHER FORECAST
JI Weather Forecast.
PD DEC
PY 2011
VL 26
IS 6
BP 1092
EP 1092
DI 10.1175/WAF-D-11-00091.1
PG 1
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 864UC
UT WOS:000298264600021
ER
PT J
AU Lorenz, RD
Jackson, BK
Barnes, JW
Spitale, JN
Radebaugh, J
Baines, KH
AF Lorenz, Ralph D.
Jackson, Brian K.
Barnes, Jason W.
Spitale, Joseph N.
Radebaugh, Jani
Baines, Kevin H.
TI Meteorological Conditions at Racetrack Playa, Death Valley National
Park: Implications for Rock Production and Transport
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID SLIDING ROCKS; CALIFORNIA; BASIN
AB Three decades of weather records at meteorological stations near Death Valley National Park are analyzed in an attempt to gauge the frequency of conditions that might form and erase the famous trails of wind-blown rocks in the mud of Racetrack Playa. Trail formation requires the playa to be wet, followed by strong winds and/or freezing conditions. Weather records are compared with a limited set of meteorological data that were acquired in situ at the playa over three winters and that indicate freezing on 50, 29, and 15 nights during the winters of 2007/08-09/10, respectively, as well as with-the hydrological condition of the playa as determined by time-lapse cameras that observed flooding over similar to 1, similar to 5, and similar to 40 days, respectively, during those winters. Measurements at the nearby Panamint and Hunter Mountain stations are found to be a useful, if imperfect (similar to 50%), indicator of Racetrack Playa conditions and give some features of Racetrack Playa's micrometeorological behavior. Wind speed probability distributions suggest that winds that are fast enough to cause unassisted rock motion are rare and therefore that freezing of water on the playa has a role in a significant fraction of movement events.
C1 [Lorenz, Ralph D.] Johns Hopkins Univ, Dept Space, Appl Phys Lab, Laurel, MD 21046 USA.
[Jackson, Brian K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID USA.
[Spitale, Joseph N.] Space Sci Inst, Boulder, CO USA.
[Radebaugh, Jani] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
[Baines, Kevin H.] Univ Wisconsin, Madison, WI USA.
RP Lorenz, RD (reprint author), Johns Hopkins Univ, Dept Space, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 21046 USA.
EM ralph.lorenz@jhuapl.edu
RI Barnes, Jason/B-1284-2009; Lorenz, Ralph/B-8759-2016
OI Barnes, Jason/0000-0002-7755-3530; Lorenz, Ralph/0000-0001-8528-4644
FU NASA; Cassini Radar (RADAR); Geological Society of America; NASA Lunar
and Planetary Sciences Academy
FX The datalogging and time-lapse experiments by RL were funded in part by
the NASA Applied Information Systems Research (AISR) program, and other
visits to the playa were supported in part by the Cassini Radar (RADAR)
program. BJK acknowledges a research grant from the Geological Society
of America and discretionary support from the director of the Lunar and
Planetary Laboratory of The University of Arizona. We thank David Choi
and Catherine Neish for assistance in the field. We are grateful for the
assistance of David Ek, wilderness resources coordinator at Death Valley
National Park, in conducting the in situ measurements. The authors
gratefully acknowledge Cynthia Cheung and the NASA Lunar and Planetary
Sciences Academy for support of the publication of this work. We thank
three anonymous reviewers for their careful reading of the paper and for
suggestions that led to its improvement.
NR 19
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U1 0
U2 17
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD DEC
PY 2011
VL 50
IS 12
BP 2361
EP 2375
DI 10.1175/JAMC-D-11-075.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 861LD
UT WOS:000298019500001
ER
PT J
AU Mlynczak, PE
Smith, GL
Doelling, DR
AF Mlynczak, Pamela E.
Smith, G. Louis
Doelling, David R.
TI The Annual Cycle of Earth Radiation Budget from Clouds and the Earth's
Radiant Energy System (CERES) Data
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID 10-YEAR DATA SET; INTERANNUAL VARIATIONS; EMITTED RADIATION;
SOLAR-RADIATION; DECONVOLUTION
AB The seasonal cycle of the Earth radiation budget is investigated by use of data from the Clouds and the Earth's Radiant Energy System (CERES). Monthly mean maps of reflected solar flux and Earth-emitted flux on a 10 equal-angle grid are used for the study. The seasonal cycles of absorbed solar radiation (ASR), outgoing longwave radiation (OLR), and net radiation are described by use of principal components for the time variations, for which the corresponding geographic variations are the empirical orthogonal functions. Earth's surface is partitioned into land and ocean for the analysis. The first principal component describes more than 95% of the variance in the seasonal cycle of ASR and the net radiation fluxes and nearly 90% of the variance of OLR over land. Because one term can express so much of the variance, principal component analysis is very useful to describe these seasonal cycles. The annual cycles of ASR are about 100 W m(-2) over land and ocean, but the amplitudes of OLR are about 27 W m(-2) over land and 15 W m(-2) over ocean. The magnitude of OLR and its time lag relative to that of ASR are important descriptors of the climate system and are computed for the first principal components. OLR lags ASR by about 26 days over land and 42 days over ocean. The principal components are useful for comparing the observed radiation budget with that computed by a model.
C1 [Doelling, David R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Mlynczak, Pamela E.; Smith, G. Louis] Sci Syst & Applications Inc, Hampton, VA USA.
RP Smith, GL (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM george.l.smith@nasa.gov
FU NASA Science Mission Directorate through Langley Research Center
FX The authors gratefully acknowledge support by the CERES program from the
NASA Science Mission Directorate through Langley Research Center to
Science Systems and Applications, Inc. They also acknowledge the CERES
project at NASA Langley for access to the dataset. They thank the
reviewers for their insightful comments and suggestions, which have
improved this paper.
NR 17
TC 6
Z9 7
U1 0
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD DEC
PY 2011
VL 50
IS 12
BP 2490
EP 2503
DI 10.1175/JAMC-D-11-050.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 861LD
UT WOS:000298019500009
ER
PT J
AU Herrmann, SM
Mohr, KI
AF Herrmann, Stefanie M.
Mohr, Karen I.
TI A Continental-Scale Classification of Rainfall Seasonality Regimes in
Africa Based on Gridded Precipitation and Land Surface Temperature
Products
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID DENSITY GAUGE DATASET; WEST-AFRICA; CLIMATE-CHANGE; UNITED-STATES;
EAST-AFRICA; VARIABILITY; VALIDATION; TRMM; MANAGEMENT; SATELLITE
AB A classification of rainfall seasonality regimes in Africa was derived from gridded rainfall and land surface temperature products. By adapting a method that goes back to Walter and Lieth's approach of presenting climatic diagrams, relationships between estimated rainfall and temperature were used to determine the presence and pattern of humid, arid, and dry months. The temporal sequence of humid, arid, and dry months defined nonseasonal as well as single-, dual-, and multiple-wet-season regimes with one or more rainfall peaks per wet season. The use of gridded products resulted in a detailed, spatially continuous classification for the entire African continent at two different spatial resolutions, which compared well to local-scale studies based on station data. With its focus on rainfall patterns at fine spatial scales, this classification is complementary to coarser and more genetic classifications based on atmospheric driving forces. An analysis of the stability of the resulting seasonality regimes shows areas of relatively high year-to-year stability in the single-wet-season regimes and areas of lower year-to-year stability in the dual- and multiple-wet-season regimes as well as in transition zones.
C1 [Herrmann, Stefanie M.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Herrmann, Stefanie M.] Sci Syst & Applications Inc, Greenbelt, MD USA.
[Mohr, Karen I.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Mohr, KI (reprint author), NASA GSFC, Atmospheres Lab, Code 613-1, Greenbelt, MD 20771 USA.
EM karen.mohr-l@nasa.gov
RI Mohr, Karen/E-4331-2012
FU NASA
FX This work was funded by the NASA Precipitation Measuring Mission. The
GPCP and TMPA products were developed by NASA/GSFC for the GEWEX Global
Precipitation Climatology Project and the Tropical Rainfall Measuring
Mission, respectively. The MODIS data products were obtained from the
Warehouse Inventory Search Tool (WIST), maintained by the EOSDIS,
NASA/GSFC. We consulted with George Huffman and David Bolvin (GSFC),
Beth Mohr (Brandeis), and Andrew Comrie (The University of Arizona). We
also acknowledge the three anonymous reviewers, whose comments helped to
improve this manuscript.
NR 45
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U1 0
U2 17
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD DEC
PY 2011
VL 50
IS 12
BP 2504
EP 2513
DI 10.1175/JAMC-D-11-024.1
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 861LD
UT WOS:000298019500010
ER
PT J
AU Kara, K
Balakumar, P
Kandil, OA
AF Kara, Kursat
Balakumar, Ponnampalam
Kandil, Osama A.
TI Effects of Nose Bluntness on Hypersonic Boundary-Layer Receptivity and
Stability over Cones
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT AIAA 37th Fluid Dynamics Conference
CY JUN 25-28, 2007
CL Miami, FL
SP AIAA
ID TRANSITION
AB The receptivity to freestream acoustic disturbances and the stability properties of hypersonic boundary layers are numerically investigated for boundary-layer flows over a 5 straight cone at a freestream Mach number of 6.0. To compute the shock and the interaction of the shock with the instability waves, the Navier-Stokes equations in axisymmetric coordinates were solved. In the governing equations, inviscid and viscous flux vectors are discretized using a fifth-order accurate weighted-essentially-non-oscillatory scheme. A third-order accurate total-variation-diminishing Runge-Kutta scheme is employed for time integration. After the mean flow field is computed, disturbances are introduced at the upstream end of the computational domain. The appearance of instability waves near the nose region and the receptivity of the boundary layer with respect to slow mode acoustic waves are investigated. Computations confirm the stabilizing effect of nose bluntness and the role of the entropy layer in the delay of boundary-layer transition. The current solutions, compared with experimental observations and other computational results, exhibit good agreement.
C1 [Kara, Kursat; Kandil, Osama A.] Old Dominion Univ, Dept Aerosp Engn, Norfolk, VA 23529 USA.
[Balakumar, Ponnampalam] NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23581 USA.
RP Kara, K (reprint author), Old Dominion Univ, Dept Aerosp Engn, Norfolk, VA 23529 USA.
EM kursat.kara@kustar.ac.ae
RI KARA, Kursat/F-2462-2011
OI KARA, Kursat/0000-0002-2788-0234
NR 25
TC 8
Z9 9
U1 0
U2 19
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 DEC
PY 2011
VL 49
IS 12
BP 2593
EP 2606
DI 10.2514/1.J050032
PG 14
WC Engineering, Aerospace
SC Engineering
GA 860SO
UT WOS:000297968200001
ER
PT J
AU Spear, AD
Priest, AR
Veilleux, MG
Ingraffea, AR
Hochhalter, JD
AF Spear, Ashley D.
Priest, Amanda R.
Veilleux, Michael G.
Ingraffea, Anthony R.
Hochhalter, Jacob D.
TI Surrogate Modeling of High-Fidelity Fracture Simulations for Real-Time
Residual-Strength Predictions
SO AIAA JOURNAL
LA English
DT Article
ID NEURAL-NETWORKS; CRACK-GROWTH; FINITE-ELEMENT; DAMAGE; IDENTIFICATION;
CRITERION; PANELS
AB A surrogate-model methodology is described for real-time prediction of the residual strength of flight structures with discrete-source damage. Starting with design of experiment, an artificial neural network is developed that takes discrete-source damage parameters as input and then outputs a prediction of the structural residual strength. Target residual-strength values used to train the artificial neural network are derived from three-dimensional finite-element-based fracture simulations. A residual-strength test of a metallic integrally stiffened panel is simulated to show that crack growth and residual strength are determined more accurately in discrete-source damage cases by using an elastic plastic fracture framework rather than a linear elastic fracture-mechanics-based method. Improving accuracy of the residual-strength training data would, in turn, improve the accuracy of the surrogate model. When combined, the surrogate-model methodology and high-fidelity fracture simulation framework provide useful tools for adaptive flight technology.
C1 [Spear, Ashley D.; Priest, Amanda R.; Veilleux, Michael G.; Ingraffea, Anthony R.] Cornell Univ, Sch Civil & Environm Engn, Ithaca, NY 14853 USA.
[Hochhalter, Jacob D.] NASA, Langley Res Ctr, Durabil & Damage Tolerance Branch, Hampton, VA 23681 USA.
RP Spear, AD (reprint author), Cornell Univ, Sch Civil & Environm Engn, 640 Rhodes Hall, Ithaca, NY 14853 USA.
FU NASA [NNX08AC50A]
FX The authors express gratitude to Robert Bucci and Mark James of Alcoa
for providing valuable discussions and experimental details from the
integrally stiffened panel test program. Thanks also to Wilkins Aquino
for providing guidance in the surrogate-modeling aspect of this work.
Funding was provided by NASA under contract NNX08AC50A, with technical
oversight provided by Edward Glaessgen and Thiagarajan Krishnamurthy of
NASA Langley Research Center.
NR 56
TC 0
Z9 0
U1 0
U2 8
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 DEC
PY 2011
VL 49
IS 12
BP 2770
EP 2782
DI 10.2514/1.J051159
PG 13
WC Engineering, Aerospace
SC Engineering
GA 860SO
UT WOS:000297968200016
ER
PT J
AU Chang, LS
Strand, CL
Jeffries, JB
Hanson, RK
Diskin, GS
Gaffney, RL
Capriotti, DP
AF Chang, Leyen S.
Strand, Christopher L.
Jeffries, Jay B.
Hanson, Ronald K.
Diskin, Glenn S.
Gaffney, Richard L.
Capriotti, Diego P.
TI Supersonic Mass-Flux Measurements via Tunable Diode Laser Absorption and
Nonuniform Flow Modeling
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 49th AIAA Aerospace Sciences Meeting/New Horizons Forum and Aerospace
Exposition
CY JAN 03-07, 2011
CL Orlando, FL
SP AIAA
ID WAVELENGTH-MODULATION SPECTROSCOPY; WATER-VAPOR; GAS TEMPERATURE;
SENSOR; COMBUSTOR; PRESSURE
AB Measurements of mass flux are obtained in a vitiated supersonic ground-test facility using a sensor based on line-of-sight diode laser absorption of water vapor. Mass flux is determined from the product of measured velocity and density. The relative Doppler shift of an absorption transition for beams directed upstream and downstream in the flow is used to measure velocity. Temperature is determined from the ratio of absorption signals of two transitions (lambda(1) = 1349 nm and lambda(2) = 1341.5 nm) and is coupled with a facility pressure measurement to obtain density. The sensor exploits wavelength-modulation spectroscopy with second-harmonic detection for large signal-to-noise ratios and normalization with the 1f signal for rejection of non-absorption-related transmission fluctuations. The sensor line of sight is translated both vertically and horizontally across the test section for spatially resolved measurements. Time-resolved measurements of mass flux are used to assess the stability of flow conditions produced by the facility. Measurements of mass flux are within 1.5% of the value obtained using a facility predictive code. The distortion of the wavelength-modulation spectroscopy lineshape caused by boundary layers along the laser line of sight is examined and the subsequent effect on the measured velocity is discussed. A method for correcting measured velocities for flow nonuniformities is introduced and application of this correction brings measured velocities within 4 m/s of the predicted value in a 1630 m/s flow.
C1 [Chang, Leyen S.; Strand, Christopher L.; Jeffries, Jay B.; Hanson, Ronald K.] Stanford Univ, Dept Mech Engn, High Temp Gasdynam Lab, Stanford, CA 94305 USA.
[Diskin, Glenn S.] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23681 USA.
[Gaffney, Richard L.; Capriotti, Diego P.] NASA, Langley Res Ctr, Hyperson Airbreathing Prop Branch, Hampton, VA 23681 USA.
RP Chang, LS (reprint author), Stanford Univ, Dept Mech Engn, High Temp Gasdynam Lab, Stanford, CA 94305 USA.
NR 17
TC 10
Z9 16
U1 0
U2 9
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD DEC
PY 2011
VL 49
IS 12
BP 2783
EP 2791
DI 10.2514/1.J051118
PG 9
WC Engineering, Aerospace
SC Engineering
GA 860SO
UT WOS:000297968200017
ER
PT J
AU Gorham, PW
Baginski, FE
Allison, P
Liewer, KM
Miki, C
Hill, B
Varner, GS
AF Gorham, P. W.
Baginski, F. E.
Allison, P.
Liewer, K. M.
Miki, C.
Hill, B.
Varner, G. S.
TI The ExaVolt Antenna: A large-aperture, balloon-embedded antenna for
ultra-high energy particle detection
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Neutrinos; Cosmic-rays
ID GAMMA-RAY BURSTS; COSMIC-RAYS; NEUTRINO; EMISSION; ACCELERATION;
RADIATION; MEMBRANES; SPECTRUM; CHARGE; WAVES
AB We describe the scientific motivation, experimental basis, design methodology, and simulated performance of the ExaVolt Antenna (EVA) mission, and planned ultra-high energy (UHE) particle observatory under development for NASA's suborbital super-pressure balloon program in Antarctica. EVA will improve over ANITA's integrated totals - the current state-of-the-art in UHE suborbital payloads - by 1-2 orders of magnitude in a single flight. The design is based on a novel application of toroidal reflector optics which utilizes a super-pressure balloon surface, along with a feed-array mounted on an inner membrane, to create an ultra-large radio antenna system with a synoptic view of the Antarctic ice sheet below it. Radio impulses arise via the Askaryan effect when UHE neutrinos interact within the ice, or via geosynchrotron emission when UHE cosmic rays interact in the atmosphere above the continent. EVA's instantaneous antenna aperture is estimated to be several hundred m(2) for detection of these events within a 150-600 MHz band. For standard cosmogenic UHE neutrino models, EVA should detect of order 30 events per flight in the EeV energy regime. For UHE cosmic rays, of order 15,000 geosynchrotron events would be detected in total, several hundred above 10 EeV, and of order 60 above the GZK cutoff energy. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Gorham, P. W.; Allison, P.; Miki, C.; Hill, B.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Baginski, F. E.] George Washington Univ, Dept Math, Washington, DC 20052 USA.
[Liewer, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Gorham, PW (reprint author), Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
EM gorham@phys.hawaii.edu
FU NASA's Balloon Program Office and Columbia Scientific Balloon Facility;
Department of Energy's Office of Science
FX We thank NASA's Balloon Program Office and Columbia Scientific Balloon
Facility, and the Department of Energy's Office of Science for their
support of these efforts. We also thank Julia Fiedler and Germano
Zerbini for their excellent work on the antenna scale models.
NR 56
TC 20
Z9 20
U1 0
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD DEC
PY 2011
VL 35
IS 5
BP 242
EP 256
DI 10.1016/j.astropartphys.2011.08.004
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 853OB
UT WOS:000297434500004
ER
PT J
AU D'Allura, A
Kulkarni, S
Carmichael, GR
Finardi, S
Adhikary, B
Wei, C
Streets, D
Zhang, Q
Pierce, RB
Al-Saadi, JA
Diskin, G
Wennberg, P
AF D'Allura, Alessio
Kulkarni, Sarika
Carmichael, Gregory R.
Finardi, Sandro
Adhikary, Bhupesh
Wei, Chao
Streets, David
Zhang, Qiang
Pierce, Robert B.
Al-Saadi, Jassim A.
Diskin, Glenn
Wennberg, Paul
TI Meteorological and air quality forecasting using the WRF-STEM model
during the 2008 ARCTAS field campaign
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article; Proceedings Paper
CT 7th International Conference on Air Quality - Science and Application
CY MAR 24-27, 2009
CL Istanbul, TURKEY
DE ARCTAS; Arctic; Air quality forecasting; Chemical weather
ID DEPOSITION; KNOWLEDGE; CHEMISTRY; SULFATE; MISSION
AB In this study, the University of Iowa's Chemical Weather Forecasting System comprising meteorological predictions using the WRF model, and off-line chemical weather predictions using tracer and full chemistry versions of the STEM model, designed to support the flight planning during the ARCTAS 2008 mission is described and evaluated. The system includes tracers representing biomass burning and anthropogenic emissions from different geographical emissions source regions, as well as air mass age indicators. We demonstrate how this forecasting system was used in flight planning and in the interpretation of the experimental data obtained through the case study of the summer mission ARCTAS DC-8 flight executed on July 9 2008 that sampled near the North Pole. The comparison of predicted meteorological variables including temperature, pressure, wind speed and wind direction against the flight observations shows that the WRF model is able to correctly describe the synoptic circulation and cloud coverage in the Arctic region The absolute values of predicted CO match the measured CO closely suggesting that the STEM model is able to capture the variability in observations within the Arctic region. The time altitude cross sections of source region tagged CO tracers along the flight track helped in identifying biomass burning (from North Asia) and anthropogenic (largely China) as major sources contributing to the observed CO along this flight. The difference between forecast and post analysis biomass burning emissions can lead to significant changes (similar to 10-50%) in primary CO predictions reflecting the large uncertainty associated with biomass burning estimates and the need to reduce this uncertainty for effective flight planning. (C) 2011 Elsevier ltd. All rights reserved.
C1 [D'Allura, Alessio; Finardi, Sandro] ARIANET, I-20128 Milan, Italy.
[Kulkarni, Sarika; Carmichael, Gregory R.; Adhikary, Bhupesh; Wei, Chao] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA USA.
[Streets, David; Zhang, Qiang] Argonne Natl Lab, Argonne, IL 60439 USA.
[Pierce, Robert B.] NOAA, NESDIS, Madison, WI USA.
[Al-Saadi, Jassim A.; Diskin, Glenn] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Wennberg, Paul] CALTECH, Pasadena, CA 91125 USA.
RP D'Allura, A (reprint author), ARIANET, Via Gilino 9, I-20128 Milan, Italy.
EM a.dallura@aria-net.it
RI Wennberg, Paul/A-5460-2012; Pierce, Robert Bradley/F-5609-2010; Zhang,
Qiang/D-9034-2012; wei, chao/E-4379-2011;
OI Pierce, Robert Bradley/0000-0002-2767-1643; Finardi,
Sandro/0000-0002-9772-785X; Streets, David/0000-0002-0223-1350
FU NASA [NNX08AH56G]
FX We would like to thank the ARCTAS Measurement Team for permission in
using the measurements, CGRER and teh University of Iowa. This work was
supported in part by NASA grant NNX08AH56G. We would like to acknowledge
Space Science and Engineering Center, University of Wisconsin-Madison,
WI, USA for providing the cloud cover satellite composite images
centered over the Arctic region.
NR 28
TC 5
Z9 5
U1 3
U2 16
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 DEC
PY 2011
VL 45
IS 38
BP 6901
EP 6910
DI 10.1016/j.atmosenv.2011.02.073
PG 10
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 854IT
UT WOS:000297488900008
ER
PT J
AU Helled, R
Anderson, JD
Schubert, G
Stevenson, DJ
AF Helled, Ravit
Anderson, John D.
Schubert, Gerald
Stevenson, David J.
TI Jupiter's moment of inertia: A possible determination by Juno
SO ICARUS
LA English
DT Article
DE Jupiter; Jupiter, Interior; Interiors
ID PLANETS; MODELS; SATELLITES; INTERIORS; NEPTUNE; HELIUM; SATURN
AB The moment of inertia of a giant planet reveals important information about the planet's internal density structure and this information is not identical to that contained in the gravitational moments. The forthcoming Juno mission to Jupiter might determine Jupiter's normalized moment of inertia NMoI = C/MR2 by measuring Jupiter's pole precession and the Lense-Thirring acceleration of the spacecraft (C is the axial moment of inertia, and M and R are Jupiter's mass and mean radius, respectively). We investigate the possible range of NMoI values for Jupiter based on its measured gravitational field using a simple core/envelope model of the planet assuming that J(2) and J(4) are perfectly known and are equal to their measured values. The model suggests that for fixed values of J(2) and J(4) a range of NMoI values between 0.2629 and 0.2645 can be found. The Radau-Darwin relation gives a NMoI value that is larger than the model values by less than 1%. A low NMoI of similar to 0.236, inferred from a dynamical model (Ward, W.R., Canup, R.M. [2006]. Astrophys. J. 640, L91-L94) is inconsistent with this range, but the range is model dependent. Although we conclude that the NMoI is tightly constrained by the gravity coefficients, a measurement of Jupiter's NMoI to a few tenths of percent by Juno could provide an important constraint on Jupiter's internal structure. We carry out a simplified assessment of the error involved in Juno's possible determination of Jupiter's NMoI. (C) Elsevier Inc. All rights reserved.
C1 [Helled, Ravit] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel.
[Anderson, John D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schubert, Gerald] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Stevenson, David J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA.
RP Helled, R (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel.
EM r.helled@gmail.com
NR 42
TC 21
Z9 21
U1 1
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD DEC
PY 2011
VL 216
IS 2
BP 440
EP 448
DI 10.1016/j.icarus.2011.09.016
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 855MH
UT WOS:000297568000007
ER
PT J
AU Clark, BE
Binzel, RP
Howell, ES
Cloutis, EA
Ockert-Bell, M
Christensen, P
Barucci, MA
DeMeo, F
Lauretta, DS
Connolly, H
Soderberg, A
Hergenrother, C
Lim, L
Emery, J
Mueller, M
AF Clark, Beth Ellen
Binzel, Richard P.
Howell, Ellen S.
Cloutis, Edward A.
Ockert-Bell, Maureen
Christensen, Phil
Barucci, Maria Antonietta
DeMeo, Francesca
Lauretta, Dante S.
Connolly, Harold, Jr.
Soderberg, Alicia
Hergenrother, Carl
Lim, Lucy
Emery, Josh
Mueller, Michael
TI Asteroid (101955) 1999 RQ36: Spectroscopy from 0.4 to 2.4 mu m and
meteorite analogs
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids, Composition
ID NEAR-EARTH ASTEROIDS; CARBONACEOUS CHONDRITES; REFLECTANCE SPECTRA;
WATER; ORGANICS; SURFACE; ICE
AB We present reflectance spectra from 0.4 to 2.4 mu m of Asteroid (101955) 1999 RQ36, the target of the OSIRIS-REx spacecraft mission. The visible spectral data were obtained at the McDonald Observatory 2.1-m telescope with the ES2 spectrograph. The infrared spectral data were obtained at the NASA Infrared Telescope Facility using the SpeX instrument. The average visible spectrum is combined with the average near-infrared wavelength spectrum to form a composite spectrum. We use three methods to constrain the compositional information in the composite spectrum of Asteroid (101955) 1999 RQ36 (hereafter RQ36). First, we perform a least-squares search for meteorite spectral analogs using 15,000 spectra from the RELAB database. Three most likely meteorite analogs are proposed based on the least-squares search. Next, six spectral parameters are measured for RQ36 and their values are compared with the ranges in parameter values of the carbonaceous chondrite meteorite classes. A most likely meteorite analog group is proposed based on the depth of overlap in parameter values. The results of the least-squares search and the parametric comparisons point to CIs and/or CMs as the most likely meteorite analogs for RQ36, and COs and CHs as the least likely. RQ36 has a spectrally "blue" continuum slope that is also observed in carbonaceous chondrites containing magnetite. We speculate that RQ36 is composed of a "CM 1"-like material. Finally, we compare RQ36 to other B-type asteroids measured by Clark et al. (Clark, B.E. et al. [2010]. J. Geophys. Res. 115, E06005). The results of this comparison are inconclusive. RQ36 is comparable to Themis spectral properties in terms of its albedo, visible spectrum, and near-infrared spectrum from 1.1 to 1.45 mu m. However, RQ36 is more similar to Pallas in terms of its near-infrared spectrum from 1.6 to 2.3 mu m. Thus it is possible that B-type asteroids form a spectral continuum and that RQ36 is a transitional object, spectrally intermediate between the two end-members. This is particularly interesting because Asteroid 24 Themis was recently discovered to have H(2)O ice on the surface (Rivkin, A., Emery, J. [2010]. Nature 464, 1322-1323; Campins, H. et al. [2010a]. Nature 464, 1320-1321). (C) 2011 Elsevier Inc. All rights reserved.
C1 [Clark, Beth Ellen; Ockert-Bell, Maureen] Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA.
[Binzel, Richard P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Howell, Ellen S.] Arecibo Observ, Arecibo, PR 00612 USA.
[Cloutis, Edward A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
[Christensen, Phil] Arizona State Univ, Tempe, AZ 85287 USA.
[Barucci, Maria Antonietta; DeMeo, Francesca] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92190 Meudon, France.
[Lauretta, Dante S.; Hergenrother, Carl] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Connolly, Harold, Jr.] CUNY, Plainfield, NJ 07060 USA.
[Soderberg, Alicia] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Lim, Lucy] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Emery, Josh] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Mueller, Michael] Observ Cote Azur, Lab Cassiopee UMR 6202, F-06304 Nice 4, France.
RP Clark, BE (reprint author), Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA.
EM bclark@ithaca.edu
RI Lim, Lucy/C-9557-2012
OI Lim, Lucy/0000-0002-9696-9654
FU Observatory of Paris
FX This manuscript benefited from reviews by Andrew S. Rivkin and an
anonymous reviewer. B.E.C. gratefully acknowledges support from the
Observatory of Paris. We thank the staff of the NASA Infrared Telescope
Facility (IRTF), including Paul Sears, Bill Golisch, and Dave Griep for
excellent telescope operation assistance. This work benefited from
conversations with Marcello Fulchignoni, Sonia Fornasier, Jason Dworkin,
Vicky Hamilton, Harold Connolly Jr., and the entire OSIRIS-REx team.
Takahiro Hiroi helped with RELAB data access, and this paper uses a
number of spectra measured by Takahiro Hiroi, Michael Gaffey, and Conel
Alexander.
NR 39
TC 45
Z9 45
U1 0
U2 18
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 DEC
PY 2011
VL 216
IS 2
BP 462
EP 475
DI 10.1016/j.icarus.2011.08.021
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 855MH
UT WOS:000297568000009
ER
PT J
AU Koskinen, TT
Yelle, RV
Snowden, DS
Lavvas, P
Sandel, BR
Capalbo, FJ
Benilan, Y
West, RA
AF Koskinen, T. T.
Yelle, R. V.
Snowden, D. S.
Lavvas, P.
Sandel, B. R.
Capalbo, F. J.
Benilan, Y.
West, R. A.
TI The mesosphere and thermosphere of Titan revealed by Cassini/UVIS
stellar occultations
SO ICARUS
LA English
DT Article
DE Titan; Occultations; Atmospheres, Structure
ID ULTRAVIOLET IMAGING SPECTROGRAPH; PHOTOABSORPTION CROSS-SECTIONS;
UPPER-ATMOSPHERE; COUPLING PHOTOCHEMISTRY; HAZE FORMATION;
GRAVITY-WAVES; TEMPERATURE; MODEL; CHEMISTRY; PROFILES
AB Stellar occultations observed by the Cassini/UVIS instrument provide unique data that probe the mesosphere and thermosphere of Titan at altitudes between 400 and 1400 km. This region is a site of complex photochemistry that forms hydrocarbon and nitrile species, and plays a crucial role in the formation of the organic hazes observed in the stratosphere, but has yet to be adequately characterized. We analyzed publicly available data obtained between flybys Tb in December 2004 and T58 in July 2009, with an emphasis on two stable occultations obtained during flybys T41 and 153. We derived detailed density profiles for CH4, C2H2, C2H4, C4H2, HCN, HC3N and C6H6 between similar to 400 and 1200 km and extinction coefficients for aerosols between 400 and 900 km. Our analysis reveals the presence of extinction layers in the occultation data that are associated with large perturbations in the density profiles of the gaseous species and extinction profiles of the aerosols. These relatively stable features vary in appearance with location and change slowly over time. In particular, we identify a sharp extinction layer between 450 and 550 km that coincides with the detached haze layer. In line with recent images obtained by Cassini/ISS, the altitude of this layer changes rapidly around the equinox in 2009. Our results point to unexpected complexity that may have significant consequences for the dynamics and physical processes taking place in the upper atmosphere of Titan. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Koskinen, T. T.; Yelle, R. V.; Snowden, D. S.; Lavvas, P.; Sandel, B. R.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Capalbo, F. J.; Benilan, Y.] Univ Paris, LISA, F-94010 Creteil, France.
[Capalbo, F. J.; Benilan, Y.] Univ Est Creteil, LISA, F-94010 Creteil, France.
[Capalbo, F. J.; Benilan, Y.] Univ Paris Diderot, LISA, F-94010 Creteil, France.
[West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Koskinen, TT (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA.
EM tommi@lpl.arizona.edu
FU NASA [NNX09AD14G, NNX09AB58G]
FX We thank B. Semonov for extensive advice on using the SPICE routines and
libraries to calculate the occultation geometry. We thank Greg Holsclaw
and William McClintock for communications regarding the properties of
the Cassini/UVIS instrument. We also thank D. Strobel, P. Rannou and I.
Muller-Wodarg for particularly fruitful conversations, and R. Vervack
for providing the Voyager/UVS results in a convenient form. We thank the
UVIS team for inspiration and for making this work possible. This
research was supported by NASA's Cassini Data Analysis Program through
Grant NNX09AD14G and Planetary Atmospheres Program through Grant
NNX09AB58G.
NR 63
TC 45
Z9 45
U1 0
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD DEC
PY 2011
VL 216
IS 2
BP 507
EP 534
DI 10.1016/j.icarus.2011.09.022
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 855MH
UT WOS:000297568000013
ER
PT J
AU Charnoz, S
Crida, A
Castillo-Rogez, JC
Lainey, V
Dones, L
Karatekin, O
Tobie, G
Mathis, S
Le Poncin-Lafitte, C
Salmon, J
AF Charnoz, Sebastien
Crida, Aurelien
Castillo-Rogez, Julie C.
Lainey, Valery
Dones, Luke
Karatekin, Ozgur
Tobie, Gabriel
Mathis, Stephane
Le Poncin-Lafitte, Christophe
Salmon, Julien
TI Accretion of Saturn's mid-sized moons during the viscous spreading of
young massive rings: Solving the paradox of silicate-poor rings versus
silicate-rich moons
SO ICARUS
LA English
DT Article
DE Saturn, Rings; Satellites, Formation; Origin, Solar System
ID OUTER SOLAR-SYSTEM; SATELLITE SYSTEMS; GIANT PLANETS; REGULAR
SATELLITES; TIDAL DISSIPATION; A-RING; EVOLUTION; BOMBARDMENT;
MIGRATION; MOONLETS
AB The origin of Saturn's inner mid-sized moons (Mimas, Enceladus, Tethys, Dione and Rhea) and Saturn's rings is debated. Charnoz et al. [Charnoz, S., Salmon J., Crida A., 2010. Nature 465, 752-754] introduced the idea that the smallest inner moons could form from the spreading of the rings' edge while Salmon et al. [Salmon, J., Charnoz, S., Crida, A., Brahic, A., 2010. Icarus 209, 771-7851 showed that the rings could have been initially massive, and so was the ring's progenitor itself. One may wonder if the mid-sized moons may have formed also from the debris of a massive ring progenitor, as also suggested by Canup [Canup, R., 2010. Nature 468, 943-946]. However, the process driving mid-sized moon accretion from the icy debris disks has not been investigated in details. In particular, Canup's (2010) model does not seem able to explain the varying silicate contents of the mid-sized moons (from 6% to 57% in mass). Here, we explore the formation of large objects from a massive ice-rich ring (a few times Rhea's mass) and describe the fundamental properties and implications of this new process. Using a hybrid computer model, we show that accretion within massive icy rings can form all mid-sized moons from Mimas to Rhea. However in order to explain their current locations, intense dissipation within Saturn (with Q(p) < 2000) is required. Our results are consistent with a satellite origin tied to the rings formation at least 2.5 Gy ago, both compatible with either a formation concurrent to Saturn or during the Late Heavy Bombardment. Tidal heating related to high-eccentricity post-accretional episodes may induce early geological activity. If some massive irregular chunks of silicates were initially present within the rings, they would be present today inside the satellites' cores which would have accreted icy shells while being tidally expelled from the rings (via a heterogeneous accretion process). These moons may be either mostly icy, or, if they contain a significant amount of rock, already differentiated from the ice without the need for radiogenic heating. The resulting inner mid-sized moons may be significantly younger than the Solar System and a similar to 1 Gyr formation delay is possible between Mimas and Rhea. The rings resulting from this process would evolve to a state compatible with current mass estimates of Saturn's rings, and nearly devoid of silicates, apart from isolated silicate chunks coated with ice, interpreted as today Saturn's rings' propellers and ring-moons (like Pan or Daphnis). (C) 2011 Elsevier Inc. All rights reserved.
C1 [Charnoz, Sebastien; Mathis, Stephane; Salmon, Julien] Univ Paris Diderot, CEA IRFU, CNRS, Ctr Orme Merisiers,Lab AIM,UMR 7158, F-91191 Gif Sur Yvette, France.
[Crida, Aurelien] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee UMR 6202, F-06304 Nice 4, France.
[Castillo-Rogez, Julie C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lainey, Valery] UPMC, Observ Paris, IMCCE, UMR CNRS 8028, F-75014 Paris, France.
[Dones, Luke; Salmon, Julien] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Karatekin, Ozgur] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Tobie, Gabriel] Univ Nantes, UFR Sci & Tech, Lab Planetol & Geodynam, F-44322 Nantes 3, France.
[Le Poncin-Lafitte, Christophe] CNRS, Observ Paris, SyRTE, UMR 8630, F-75014 Paris, France.
RP Charnoz, S (reprint author), Univ Paris Diderot, CEA IRFU, CNRS, Ctr Orme Merisiers,Lab AIM,UMR 7158, F-91191 Gif Sur Yvette, France.
EM charnoz@cea.fr
FU CAMPUS SPATIAL grant; Institut Universitaire de France (IUF);
CEA/IRFU/SAp; EMERGENCE UPMC [EME0911]; Cassini project; French
Programme National de Planetologie (PNP)
FX We thank warmly Paul Estrada for his detailed review that helped us to
increase the quality of the paper. Part of this work was carried out at
Universite Paris Diderot with a partial funding from a CAMPUS SPATIAL
grant, as well as by Institut Universitaire de France (IUF). It was also
supported by CEA/IRFU/SAp, and by an EMERGENCE UPMC grant (Contract
Number EME0911) and by the Cassini project. Part of this work has been
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract to NASA. US Government sponsorship
acknowledged Support from the French Programme National de Planetologie
(PNP) is also acknowledged.
NR 70
TC 43
Z9 43
U1 6
U2 14
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 DEC
PY 2011
VL 216
IS 2
BP 535
EP 550
DI 10.1016/j.icarus.2011.09.017
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 855MH
UT WOS:000297568000014
ER
PT J
AU Choi, DS
Showman, AP
AF Choi, David S.
Showman, Adam P.
TI Power spectral analysis of Jupiter's clouds and kinetic energy from
Cassini
SO ICARUS
LA English
DT Article
DE Jupiter, Atmosphere; Atmospheres, Dynamics; Atmospheres, Structure
ID GREAT RED SPOT; SHALLOW-WATER TURBULENCE; 5-MICRON HOT-SPOTS; MEAN ZONAL
FLOW; 2-DIMENSIONAL TURBULENCE; MOIST CONVECTION; GIANT PLANETS; JOVIAN
ATMOSPHERE; ROTATING SPHERE; IMAGING DATA
AB We present suggestive evidence for an inverse energy cascade within Jupiter's atmosphere through a calculation of the power spectrum of its kinetic energy and its cloud patterns. Using Cassini observations, we composed full-longitudinal mosaics of Jupiter's atmosphere at several wavelengths. We also utilized image pairs derived from these observations to generate full-longitudinal maps of wind vectors and atmospheric kinetic energy within Jupiter's troposphere. We computed power spectra of the image mosaics and kinetic energy maps using spherical harmonic analysis. Power spectra of Jupiter's cloud patterns imaged at certain wavelengths resemble theoretical spectra of two-dimensional turbulence, with power-law slopes near -5/3 and -3 at low and high wavenumbers, respectively. The slopes of the kinetic energy power spectrum are also near -5/3 at low wavenumbers. At high wavenumbers, however, the spectral slopes are relatively flatter than the theoretical prediction of -3. In addition, the image mosaic and kinetic energy power spectra differ with respect to the location of the transition in slopes. The transition in slope is near planetary wavenumber 70 for the kinetic energy spectra, but is typically above 200 for the image mosaic spectra. Our results also show the importance of calculating spectral slopes from full 2D velocity maps rather than 1D zonal mean velocity profiles, since at large wavenumbers the spectra differ significantly, though at low wavenumbers, the 1D zonal and full 2D kinetic energy spectra are practically indistinguishable. Furthermore, the difference between the image and kinetic energy spectra suggests some caution in the interpretation of power spectrum results solely from image mosaics and its significance for the underlying dynamics. Finally, we also report prominent variations in kinetic energy within the equatorial jet stream that appear to be associated with the 5 mu m hotspots. Other eddies are present within the flow collar of the Great Red Spot, suggesting caution when interpreting snapshots of the flow inside these features as representative of a time-averaged state. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Choi, David S.; Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
RP Choi, DS (reprint author), NASA, ORAU, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM david.s.choi@nasa.gov
RI Choi, David/C-5215-2012
FU NASA [NNX09AD98G, NNX08AW01H]
FX We thank Boris Galperin and an anonymous referee for helpful comments
that strengthened this manuscript. Lorenzo Polvani, Peter Read, and
Robert Scott provided valuable advice for this project. We thank Ashwin
Vasavada for his work in compiling the raw Cassini images and producing
mosaics for the PDS Atmospheres node. This research was supported by a
NASA Jupiter Data Analysis Program Grant, #NNX09AD98G, as well as a NASA
Earth and Space Science Fellowship, #NNX08AW01H. Additional support was
provided by a University of Arizona TRIF Imaging Fellowship.
NR 60
TC 11
Z9 11
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 DEC
PY 2011
VL 216
IS 2
BP 597
EP 609
DI 10.1016/j.icarus.2011.10.001
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 855MH
UT WOS:000297568000018
ER
PT J
AU Li, JY
Bodewits, D
Feaga, LM
Landsman, W
A'Hearn, MF
Mutchler, MJ
Russell, CT
McFadden, LA
Raymond, CA
AF Li, Jian-Yang
Bodewits, Dennis
Feaga, Lori M.
Landsman, Wayne
A'Hearn, Michael F.
Mutchler, Max J.
Russell, Christopher T.
McFadden, Lucy A.
Raymond, Carol A.
TI Ultraviolet spectroscopy of Asteroid (4) Vesta
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Spectrophotometry; Spectroscopy; Ultraviolet
observations; Hubble Space Telescope observations
ID HUBBLE-SPACE-TELESCOPE; TRIAXIAL ELLIPSOID DIMENSIONS; ADAPTIVE OPTICS
IMAGES; REFLECTANCE PROPERTIES; ROTATIONAL POLES; ROSETTA-ALICE; 21
LUTETIA; CERES; SPECTRA; RECALIBRATION
AB We report a comprehensive review of the UV-visible spectrum and rotational lightcurve of Vesta combining new observations by Hubble Space Telescope and Swift Gamma-ray Burst Observatory with archival International Ultraviolet Explorer observations. The geometric albedos of Vesta from 220 nm to 953 nm are derived by carefully comparing these observations from various instruments at different times and observing geometries. Vesta has a rotationally averaged geometric albedo of 0.09 at 250 nm, 0.14 at 300 nm, 0.26 at 373 nm, 0.38 at 673 nm, and 0.30 at 950 nm. The linear spectral slope as measured between 240 and 320 nm in the ultraviolet displays a sharp minimum near a sub-Earth longitude of 20, and maximum in the eastern hemisphere. This is consistent with the longitudinal distribution of the spectral slope in the visible wavelength. The photometric uncertainty in the ultraviolet is similar to 20%, and in the visible wavelengths it is better than similar to 10%. The amplitude of Vesta's rotational lightcurves is 10% throughout the range of wavelengths we observed, but is smaller at 950 nm (similar to 6%) near the 1-mu m band center. Contrary to earlier reports, we found no evidence for any difference between the phasing of the ultraviolet and visible/near-infrared lightcurves with respect to sub-Earth longitude. Vesta's average spectrum between 220 and 950 nm can well be described by measured reflectance spectra of fine particle howardite-like materials of basaltic achondrite meteorites. Combining this with the in-phase behavior of the ultraviolet, visible, and near-infrared lightcurves, and the spectral slopes with respect to the rotational phase, we conclude that there is no global ultraviolet/visible reversal on Vesta. Consequently, this implies a lack of global space weathering on Vesta, as previously inferred from visible-near-infrared data. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Li, Jian-Yang; Bodewits, Dennis; Feaga, Lori M.; A'Hearn, Michael F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Landsman, Wayne; McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mutchler, Max J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Russell, Christopher T.] Univ Calif Los Angeles, IGPP, Los Angeles, CA 90095 USA.
[Russell, Christopher T.] Univ Calif Los Angeles, ESS, Los Angeles, CA 90095 USA.
[Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Li, JY (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM jyli@astro.umd.edu
RI McFadden, Lucy-Ann/I-4902-2013; Russell, Christopher/E-7745-2012;
OI McFadden, Lucy-Ann/0000-0002-0537-9975; Russell,
Christopher/0000-0003-1639-8298; Bodewits, Dennis/0000-0002-2668-7248
FU National Aeronautics and Space Administration (NASA) from the Space
Telescope Science Institute [HST-GO-12049.01-A, NAS5-26555]; Swift Guest
Investigator program; NASA [NAGW-748]
FX Support for this work was provided by the National Aeronautics and Space
Administration (NASA) through Grant HST-GO-12049.01-A from the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA Contract
NAS5-26555. We thank the Swift team for the careful and successful
planning of our observations and acknowledge support from the Swift
Guest Investigator program. A portion of this work was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. Select reflectance spectra were acquired from the
RELAB database maintained by Brown University. RELAB is a multiuser
facility operated under NASA Grant NAGW-748. JYL would like to extend
special thanks to Dr. Amanda Hendrix and Dr. Faith Vilas for the very
helpful discussions on their previous work. The authors are grateful to
the two reviewers for their critical readings of this manuscript that
have helped us clarify our conclusions and improve the manuscript
substantially.
NR 55
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U1 0
U2 5
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD DEC
PY 2011
VL 216
IS 2
BP 640
EP 649
DI 10.1016/j.icarus.2011.10.003
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 855MH
UT WOS:000297568000021
ER
PT J
AU Gariel, M
Srivastava, AN
Feron, E
AF Gariel, Maxime
Srivastava, Ashok N.
Feron, Eric
TI Trajectory Clustering and an Application to Airspace Monitoring
SO IEEE TRANSACTIONS ON INTELLIGENT TRANSPORTATION SYSTEMS
LA English
DT Article
DE Air traffic management; airspace monitoring; complexity; trajectory
clustering
AB This paper presents a framework aimed at monitoring the behavior of aircraft in a given airspace. Trajectories that constitute typical operations are determined and learned using data-driven methods. Standard procedures are used by air traffic controllers (ATCs) to guide aircraft, ensure the safety of the airspace, and maximize runway occupancy. Even though standard procedures are used by ATCs, control of the aircraft remains with the pilots, leading to large variability in the flight patterns observed. Two methods for identifying typical operations and their variability from recorded radar tracks are presented. This knowledge base is then used to monitor the conformance of current operations against operations previously identified as typical. A tool called AirTrajectoryMiner is presented, aiming at monitoring the instantaneous health of the airspace, in real time. The airspace is "healthy" when all aircraft are flying according to typical operations. A measure of complexity is introduced, measuring the conformance of current flight to typical flight patterns. When an aircraft does not conform, the complexity increases as more attention from ATC is required to ensure safe separation between aircraft.
C1 [Gariel, Maxime; Feron, Eric] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Srivastava, Ashok N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Gariel, M (reprint author), MIT, Informat & Decis Syst Lab, Cambridge, MA 02139 USA.
FU Thales Air Systems; National Aeronautics and Space Administration
[NNX08AY52A]
FX Manuscript received May 27, 2010; revised February 4, 2011 and March 6,
2011; accepted June 8, 2011. Date of publication July 22, 2011; date of
current version December 5, 2011. This work was supported in part by
Thales Air Systems and in part by the National Aeronautics and Space
Administration under Grant NNX08AY52A. The Associate Editor for this
paper was J.-P. B. Clarke.
NR 35
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Z9 48
U1 2
U2 17
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1524-9050
J9 IEEE T INTELL TRANSP
JI IEEE Trans. Intell. Transp. Syst.
PD DEC
PY 2011
VL 12
IS 4
BP 1511
EP 1524
DI 10.1109/TITS.2011.2160628
PG 14
WC Engineering, Civil; Engineering, Electrical & Electronic; Transportation
Science & Technology
SC Engineering; Transportation
GA 855TS
UT WOS:000297588500051
ER
PT J
AU Blackmore, L
Ono, M
Williams, BC
AF Blackmore, Lars
Ono, Masahiro
Williams, Brian C.
TI Chance-Constrained Optimal Path Planning With Obstacles
SO IEEE TRANSACTIONS ON ROBOTICS
LA English
DT Article
DE Autonomous agents; chance constraints; optimization under uncertainty;
probabilistic planning
ID MODEL-PREDICTIVE CONTROL; ROBUST; OPTIMIZATION
AB Autonomous vehicles need to plan trajectories to a specified goal that avoid obstacles. For robust execution, we must take into account uncertainty, which arises due to uncertain localization, modeling errors, and disturbances. Prior work handled the case of set-bounded uncertainty. We present here a chance-constrained approach, which uses instead a probabilistic representation of uncertainty. The new approach plans the future probabilistic distribution of the vehicle state so that the probability of failure is below a specified threshold. Failure occurs when the vehicle collides with an obstacle or leaves an operator-specified region. The key idea behind the approach is to use bounds on the probability of collision to show that, for linear-Gaussian systems, we can approximate the nonconvex chance-constrained optimization problem as a disjunctive convex program. This can be solved to global optimality using branch-and-bound techniques. In order to improve computation time, we introduce a customized solution method that returns almost-optimal solutions along with a hard bound on the level of suboptimality. We present an empirical validation with an aircraft obstacle avoidance example.
C1 [Blackmore, Lars] CALTECH, Jet Prop Lab, Guidance Control Anal Grp, Pasadena, CA 91109 USA.
[Ono, Masahiro; Williams, Brian C.] MIT, Cambridge, MA 02139 USA.
RP Blackmore, L (reprint author), CALTECH, Jet Prop Lab, Guidance Control Anal Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM larsblackmore@gmail.com; hiro_ono@mit.edu; williams@mit.edu
FU U.S. Government; National Science Foundation [IIS-1017992]; Boeing
Company [MIT-BA-GTA-1]; National Aeronautics and Space Administration
FX The authors would like to acknowledge the support of the U.S.
Government. Any opinions, findings, conclusions, or recommendations
expressed in this paper are those of the authors and do not necessarily
reflect the view of the sponsoring agencies. They would also like to
thank M. Kerstetter, S. Smith, R. Provine, and H. Li at Boeing Company
for their support.; This work supported in part by the National Science
Foundation under Grant IIS-1017992 and by the Boeing Company under Grant
MIT-BA-GTA-1. The work was carried out in part at the Jet Propulsion
Laboratory, California Institute of Technology, Pasadena, CA, under a
contract with the National Aeronautics and Space Administration.
NR 52
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U1 2
U2 23
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1552-3098
EI 1941-0468
J9 IEEE T ROBOT
JI IEEE Trans. Robot.
PD DEC
PY 2011
VL 27
IS 6
BP 1080
EP 1094
DI 10.1109/TRO.2011.2161160
PG 15
WC Robotics
SC Robotics
GA 858RW
UT WOS:000297821400005
ER
PT J
AU Browning, G
Carlsson, LA
Ratcliffe, JG
AF Browning, Grant
Carlsson, Leif A.
Ratcliffe, James G.
TI Modification of the edge crack torsion specimen for mode III
delamination testing. Part II - experimental study
SO JOURNAL OF COMPOSITE MATERIALS
LA English
DT Article
DE mode III delamination; test method; experimental evaluation
ID INTERLAMINAR FRACTURE; ECT TEST
AB Experimental studies of carbon/epoxy edge crack torsion specimen have been conducted using a specially designed twist test fixture. Of particular concern was verification of the recommendations expressed in the analytical part of this study (Part 1), where it was suggested that overhang (sections of specimen laying outside of the loading and support pins) in the x- and y-directions should be minimized, and fracture testing at longer delamination lengths should be avoided. The experimental test results verified that the specimens with the smallest overhang produced the most consistent delamination toughness data, G(IIIc). Specimens with large overhangs exhibited high apparent G(IIIc) values at long delamination lengths. This was most likely due to nonuniform loading and associated nonuniform delamination extension.
C1 [Ratcliffe, James G.] Natl Inst Aerosp, NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Browning, Grant; Carlsson, Leif A.] Florida Atlantic Univ, Dept Mech Engn, Boca Raton, FL 33431 USA.
RP Ratcliffe, JG (reprint author), Natl Inst Aerosp, NASA, Langley Res Ctr, Mail Code 188E, Hampton, VA 23681 USA.
EM james.g.ratcliffe@nasa.gov
FU Bell Helicopter Textron; Center for Rotorcraft Innovation (CRI);
National Rotorcraft Technology Center (NRTC), US Army Aviation and
Missile Research, Development and Engineering Center [W911W6-06-2-0002];
NRTC; CRI/Bell Helicopter
FX This research is part of a program that was partially funded by Bell
Helicopter Textron and the Center for Rotorcraft Innovation (CRI), and
partially funded by the National Rotorcraft Technology Center (NRTC), US
Army Aviation and Missile Research, Development and Engineering Center
under Technology Investment Agreement W911W6-06-2-0002, entitled
National Rotorcraft Technology Center Research Program. The authors
would like to acknowledge that this research and development was
accomplished with the support and guidance of the NRTC and CRI/Bell
Helicopter through Dr Xiaoming Li as the program lead. The drawings were
prepared by Josh Kahn, and text was prepared by Laura Thornton.
NR 10
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U1 1
U2 4
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0021-9983
J9 J COMPOS MATER
JI J. Compos Mater.
PD DEC
PY 2011
VL 45
IS 25
BP 2633
EP 2640
DI 10.1177/0021998311401115
PG 8
WC Materials Science, Composites
SC Materials Science
GA 854UK
UT WOS:000297519800004
ER
PT J
AU Ratcliffe, JG
Reeder, JR
AF Ratcliffe, James G.
Reeder, James R.
TI Sizing a single cantilever beam specimen for characterizing
facesheet-core debonding in sandwich structure
SO JOURNAL OF COMPOSITE MATERIALS
LA English
DT Article
DE sandwich structure; facesheet-core debonding; test method
ID WEAVE FABRIC COMPOSITES; FRACTURE-MECHANICS; CRACK-PROPAGATION;
INTERFACE CRACK; DELAMINATION; ADHESION; TOUGHNESS; PANELS; MODEL
AB This article details a procedure for sizing single cantilever beam (SCB) test specimens that are used to characterize facesheet-core debonding in sandwich structure. The characterization is accomplished by measuring the critical strain energy release rate, G(c), associated with the debonding process. The sizing procedure is based on an analytical representation of the SCB specimen, which models the specimen as a cantilever beam partially supported on an elastic foundation. This results in an approximate, closed-form solution for the compliance-debond length relationship of the specimen. The solution provides a series of limitations that can be imposed on the specimen dimensions to help ensure the specimen behaviour does not violate assumptions made in the derivation of the data reduction method used to calculate G(c). Application of the sizing procedure to actual sandwich systems yielded SCB specimen dimensions that would be practical for use. The method is specifically configured for incorporation into a draft testing protocol to be developed into an ASTM International testing standard.
C1 [Ratcliffe, James G.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Reeder, James R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Reeder, JR (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM james.g.ratcliffe@nasa.gov
FU NASA
FX This research was conducted at the Durability, Damage Tolerance, and
Reliability Branch, NASA Langley Research Center, VA, and funded by the
NASA Fundamental Aeronautics Program/Subsonic Rotary Wing Program.
NR 36
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U1 0
U2 4
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0021-9983
J9 J COMPOS MATER
JI J. Compos Mater.
PD DEC
PY 2011
VL 45
IS 25
BP 2669
EP 2684
DI 10.1177/0021998311401116
PG 16
WC Materials Science, Composites
SC Materials Science
GA 854UK
UT WOS:000297519800007
ER
PT J
AU Smith, EJ
AF Smith, Edward J.
TI What causes the flux excess in the heliospheric magnetic field?
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ROTATING RAREFACTION REGIONS; OPEN SOLAR FLUX; ULYSSES; LATITUDE
AB Ulysses results indicate that the total magnetic flux inside the heliosphere, Phi, can be obtained from the radial field component measured at a single spacecraft multiplied by the square of the radial distance and averaged over a solar rotation, < r(2)B(R) >. However, that result is contrary to a large increase in F with distance, called the flux excess, that has been reported by Owens et al. (2008a) and attributed to variations in solar wind speed by Lockwood et al. (2009a, 2009b). Ulysses data and a mathematical simulation are used to show that the cause of the flux excess is the replacement of B(R) by the modulus, |B(R)|. The modulus rectifies some of the large amplitude magnetic field variations normally present in measurements of BR and increases the mean, < r(2) |B(R)| > relative to < r(2)B(R) >. The variance of the magnetic fluctuations, sigma, decreases less rapidly with distance than B(R) and that produces a progressively larger error in < r(2) |B(R)| > resulting in the flux excess. The advisability of defining F in terms of |B(R)|, of using < r(2) |B(R)| > beyond 1 AU and the applicability of the Lockwood et al. (2009b) correction to < r(2) |B(R)| > are questioned.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Smith, EJ (reprint author), CALTECH, Jet Prop Lab, M-S 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM edward.j.smith@jpl.nasa.gov
FU National Aeronautics and Space Administration
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.
The analysis in this paper was motivated by the Owens et al. [2008a]
results and by discussions of the flux excess at the Third Space Climate
Symposium in Saariselka, Finland in March 2009. The two referees
provided valuable assistance. Comments from both referees were helpful.
One referee read the manuscript from a very different point of view that
I had not contemplated in the original manuscript and that led to
several very important clarifications. Joyce Wolf provided valuable
assistance with the analysis and figures.
NR 22
TC 8
Z9 8
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD DEC 1
PY 2011
VL 116
AR A12101
DI 10.1029/2011JA016521
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 856NN
UT WOS:000297649600001
ER
PT J
AU Sebree, JA
Plusquellic, DF
Zwier, TS
AF Sebree, Joshua A.
Plusquellic, David F.
Zwier, Timothy S.
TI Spectroscopic characterization of structural isomers of naphthalene:
1-Phenyl-1-butyn-3-ene
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Naphthalene isomers; Vibronic coupling; Phenylvinylacetylene
ID AB-INITIO; PHENYLACETYLENE; (E)-PHENYLVINYLACETYLENE; MECHANISMS;
TRANSITION; DENSITY; STYRENE; SYSTEM
AB Laser induced fluorescence (LIF), single vibronic level dispersed fluorescence (DFL) spectra, and high resolution rotationally resolved scans of the S(0)-S(1) transition of the C(10)H(8) isomer 1-phenyl-1-butyn-3-ene have been recorded under jet-cooled conditions. The S(0)-S(1) origin of PAV at 34922 cm(-1) is very weak. A vibronic band located 464.0 above the origin, assigned as 30(0)(1), dominates the LIF excitation spectrum, with intensity arising from vibronic coupling with the S(2) state. High resolution scans of the S(0)-S(1) origin and 3010 vibronic bands determine that the former is a 65:35 a:b hybrid band, while 30(0)(1) is a pure a-type band, confirming the role for vibronic coupling and identifying the coupled state as the S(2) state. DFL spectra of all vibronic bands in the first 800 cm(-1) of the spectrum were recorded. A near-complete assignment of the vibronic structure in both S(0) and S(1) states is obtained. Herzberg-Teller vibronic coupling is carried by two vibrations, v(28) and v(30), involving in-plane deformations of the vinylacetylene side chain, leading to Duschinsky mixing evident in the intensities of transitions in excitation and DFL spectra. Extensive Duschinsky mixing is also present among the lowest five out-of-plane vibrational modes, involving motion of the side chain. Comparison with the results of DFT B3LYP and TDDFT calculations with a 6-311+G(d,p) basis set confirm and strengthen the assignments. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Zwier, Timothy S.] Purdue Univ, Dept Chem, W Lafayette, IN 47909 USA.
[Plusquellic, David F.] NIST, Opt Technol Div, Gaithersburg, MD 20899 USA.
[Sebree, Joshua A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zwier, TS (reprint author), Purdue Univ, Dept Chem, W Lafayette, IN 47909 USA.
EM zwier@purdue.edu
RI Sebree, Josh/F-2423-2012
OI Sebree, Josh/0000-0001-9612-8532
FU NASA [NNX10AB89G]
FX The authors gratefully acknowledge support from the NASA Planetary
Atmospheres program under Grant NNX10AB89G for this research.
NR 36
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U1 0
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD DEC
PY 2011
VL 270
IS 2
BP 98
EP 107
DI 10.1016/j.jms.2011.10.001
PG 10
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 859VL
UT WOS:000297903800002
ER
PT J
AU Generazio, ER
AF Generazio, E. R.
TI Validating Design of Experiments for Determining Probability of
Detection Capability for Fracture Critical Applications
SO MATERIALS EVALUATION
LA English
DT Article
DE probability of detection; nondestructive testing
ID SYSTEMS
AB The capability of an inspection system is established by applications of various methodologies to determine the probability of detection (POD). One accepted metric of an adequate inspection system is that, for a minimum discontinuity size and all greater discontinuity sizes, there is 0.90 probability of detection with 95% confidence (90/95 POD). Directed design of experiments for probability of detection (DOEPOD) has been developed to provide an efficient and accurate nonparametric methodology that yields estimates of POD and confidence bounds for both hit-miss and signal amplitude testing. DOEPOD uses a nonparametric approach for the analysis of inspection data that does require any assumptions about the particular functional form of a POD function. The conservativeness of the DOEPOD methodology results is discussed. Validated guidelines for binomial estimation of POD for fracture critical inspection are established.
C1 Natl Aeronaut & Space Adm, Hampton, VA 23681 USA.
RP Generazio, ER (reprint author), Natl Aeronaut & Space Adm, Hampton, VA 23681 USA.
FU D W Enterprises
FX The author wishes to thank Ward D. Rummel of D & W Enterprises for his
support and recommendation, and William Q Meeker of Iowa State
University for clarifying statistical concepts and procedures, and
providing guidance on Monte Carlo testing.
NR 17
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Z9 2
U1 0
U2 2
PU AMER SOC NONDESTRUCTIVE TEST
PI COLUMBUS
PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA
SN 0025-5327
J9 MATER EVAL
JI Mater. Eval.
PD DEC
PY 2011
VL 69
IS 12
BP 1399
EP 1407
PG 9
WC Materials Science, Characterization & Testing
SC Materials Science
GA 859LI
UT WOS:000297877500007
ER
PT J
AU Yang, MJ
Braun, SA
Chen, DS
AF Yang, Ming-Jen
Braun, Scott A.
Chen, Deng-Shun
TI Water Budget of Typhoon Nari (2001)
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID HURRICANE-ANDREW 1992; INNER-CORE; PRECIPITATION EFFICIENCY; PART II;
NORBERT; MODEL; ICE
AB Although there have been many observational and modeling studies of tropical cyclones (TCs), the understanding of TCs' budgets of vapor and condensate and the changes of budgets after TCs' landfall is still quite limited. In this study, high-resolution (2-km horizontal grid size and 2-min data interval) model output from a cloud-resolving simulation of Typhoon Nari (2001) is used to examine the vapor and condensate budgets and the respective changes of the budgets after Nari's landfall on Taiwan. All budget terms are directly derived from the model except for a small residual term. For the vapor budget, while Nari is over the ocean, evaporation from the ocean surface is 11% of the inward horizontal vapor transport within 150 km of the storm center, and the net horizontal vapor convergence into the storm is 88% of the net condensation. The ocean source of water vapor in the inner core is a small portion (5.5%) of horizontal vapor import, consistent with previous studies. After landfall, Taiwan's steep terrain enhances Nari's secondary circulation significantly and produces stronger horizontal vapor import at low levels, resulting in a 22% increase in storm-total condensation. Precipitation efficiency, defined from either the large-scale or microphysics perspective, is increased 10%-20% over the outer-rainband region after landfall, in agreement with the enhanced surface rainfall over the complex terrain.
C1 [Yang, Ming-Jen; Chen, Deng-Shun] Natl Cent Univ, Dept Atmospher Sci, Chungli 320, Taiwan.
[Yang, Ming-Jen] Natl Cent Univ, Inst Hydrol & Ocean Sci, Chungli 320, Taiwan.
[Yang, Ming-Jen] Taiwan Typhoon Flood Res Inst, Chungli, Taiwan.
[Braun, Scott A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Yang, MJ (reprint author), Natl Cent Univ, Dept Atmospher Sci, 300 Chung Da Rd, Chungli 320, Taiwan.
EM mingjen@cc.ncu.edu.tw
RI Yang, Ming-Jen/F-4628-2012
OI Yang, Ming-Jen/0000-0001-6654-2791
FU National Science Council of Taiwan [NSC 97-2111-M-008-019-MY3, NSC
99-2625-M-008-005-MY3, NSC 98-2745-M-008-012-MY3]; Central Weather
Bureau [MOTC-CWB-100-M-15]
FX We appreciate two anonymous reviewers' helpful comments, which improved
the quality of this manuscript significantly. This work was supported by
the National Science Council of Taiwan under Grants NSC
97-2111-M-008-019-MY3, NSC 99-2625-M-008-005-MY3, and NSC
98-2745-M-008-012-MY3, and by the Central Weather Bureau under Grant
MOTC-CWB-100-M-15.
NR 28
TC 8
Z9 9
U1 0
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD DEC
PY 2011
VL 139
IS 12
BP 3809
EP 3828
DI 10.1175/MWR-D-10-05090.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 855ZD
UT WOS:000297603900009
ER
PT J
AU Thone, CC
Postigo, AD
Fryer, CL
Page, KL
Gorosabel, J
Aloy, MA
Perley, DA
Kouveliotou, C
Janka, HT
Mimica, P
Racusin, JL
Krimm, H
Cummings, J
Oates, SR
Holland, ST
Siegel, MH
De Pasquale, M
Sonbas, E
Im, M
Park, WK
Kann, DA
Guziy, S
Garcia, LH
Llorente, A
Bundy, K
Choi, C
Jeong, H
Korhonen, H
Kubanek, P
Lim, J
Moskvitin, A
Munoz-Darias, T
Pak, S
Parrish, I
AF Thoene, C. C.
Postigo, A. de Ugarte
Fryer, C. L.
Page, K. L.
Gorosabel, J.
Aloy, M. A.
Perley, D. A.
Kouveliotou, C.
Janka, H. T.
Mimica, P.
Racusin, J. L.
Krimm, H.
Cummings, J.
Oates, S. R.
Holland, S. T.
Siegel, M. H.
De Pasquale, M.
Sonbas, E.
Im, M.
Park, W. -K.
Kann, D. A.
Guziy, S.
Hernandez Garcia, L.
Llorente, A.
Bundy, K.
Choi, C.
Jeong, H.
Korhonen, H.
Kubanek, P.
Lim, J.
Moskvitin, A.
Munoz-Darias, T.
Pak, S.
Parrish, I.
TI The unusual gamma-ray burst GRB 101225A from a helium star/neutron star
merger at redshift 0.33
SO NATURE
LA English
DT Article
ID SUPERNOVA; GRB-060218; GALAXY; SWIFT; HOLE
AB Long gamma-ray bursts (GRBs) are the most dramatic examples of massive stellar deaths, often associated with supernovae(1). They release ultra-relativistic jets, which produce non-thermal emission through synchrotron radiation as they interact with the surrounding medium(2). Here we report observations of the unusual GRB 101225A. Its gamma-ray emission was exceptionally long-lived and was followed by a bright X-ray transient with a hot thermal component and an unusual optical counterpart. During the first 10 days, the optical emission evolved as an expanding, cooling black body, after which an additional component, consistent with a faint supernova, emerged. We estimate its redshift to be z = 0.33 by fitting the spectral-energy distribution and light curve of the optical emission with a GRB-supernova template. Deep optical observations may have revealed a faint, unresolved host galaxy. Our proposed progenitor is a merger of a helium star with a neutron star that underwent a common envelope phase, expelling its hydrogen envelope. The resulting explosion created a GRB-like jet which became thermalized by interacting with the dense, previously ejected material, thus creating the observed black body, until finally the emission from the supernova dominated. An alternative explanation is a minor body falling onto a neutron star in the Galaxy(3).
C1 [Thoene, C. C.; Gorosabel, J.; Guziy, S.; Hernandez Garcia, L.; Kubanek, P.] IAA CSIC, Granada 18008, Spain.
[Thoene, C. C.] Niels Bohr Int Acad, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Postigo, A. de Ugarte] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Fryer, C. L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Aloy, M. A.; Mimica, P.] Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain.
[Perley, D. A.; Bundy, K.; Parrish, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Sci & Technol Off, Huntsville, AL 35812 USA.
[Janka, H. T.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Racusin, J. L.; Krimm, H.; Cummings, J.; Holland, S. T.; Sonbas, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimm, H.; Holland, S. T.; Sonbas, E.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Krimm, H.; Holland, S. T.] CRESST, Columbia, MD 21044 USA.
[Oates, S. R.; De Pasquale, M.] Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Siegel, M. H.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 104, University Pk, PA 16802 USA.
[Sonbas, E.] Univ Adiyaman, Dept Phys, TR-02040 Adiyaman, Turkey.
[Im, M.; Park, W. -K.; Choi, C.] Seoul Natl Univ, Dept Phys & Astron, Ctr Explorat Origin Universe, Seoul, South Korea.
[Kann, D. A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Guziy, S.] Nikolaev Natl Univ, UA-54030 Nikolayev, Ukraine.
[Llorente, A.] ESAC, INSA, Herschel Sci Operat Ctr, Madrid 28080, Spain.
[Jeong, H.; Pak, S.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea.
[Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland.
[Kubanek, P.] Inst Phys, Prague 18000 8, Czech Republic.
[Lim, J.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi Do, South Korea.
[Moskvitin, A.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia.
[Munoz-Darias, T.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
RP Thone, CC (reprint author), IAA CSIC, Glorieta Astron S-N, Granada 18008, Spain.
EM cthoene@iaa.es
RI Kubanek, Petr/G-7209-2014; Aloy, Miguel/K-9941-2014; Korhonen,
Heidi/E-3065-2016; Racusin, Judith/D-2935-2012; Lujan Center,
LANL/G-4896-2012; Im, Myungshin/B-3436-2013; Pak, Soojong/E-2360-2013
OI Aloy, Miguel/0000-0002-5552-7681; Korhonen, Heidi/0000-0003-0529-1161;
Thone, Christina/0000-0002-7978-7648; Im, Myungshin/0000-0002-8537-6714;
FU DNRF; UK Space Agency; MICINN; ERC; DFG; CRI/NRF/MEST of Korea; Russian
government
FX This Letter is based on observations collected at CAHA/Calar Alto,
GTC/La Palma, the Liverpool Telescope at ORM/La Palma, the McDonald
Observatory at the University of Texas at Austin, and Gemini-North and
Keck on Hawaii. We thank J. S. Bloom for helping with the Keck
observations. The Dark Cosmology Centre is funded by the DNRF. K. L. P.,
S.R.O. and M.D.P. acknowledge the support of the UK Space Agency. J. G.,
S. G. and P. K. are partially supported by MICINN. M. A. A. and P. M.
are supported by an ERC starting grant. H. T. J. acknowledges support by
a DFG grant. M. I., W.-K.P., C. C., J. L. and S. P. acknowledge support
from CRI/NRF/MEST of Korea. A. M. acknowledges support from the Russian
government.
NR 21
TC 53
Z9 53
U1 1
U2 9
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD DEC 1
PY 2011
VL 480
IS 7375
BP 72
EP 74
DI 10.1038/nature10611
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 861PO
UT WOS:000298031900035
PM 22129726
ER
PT J
AU Pandey, G
Kareliya, C
Hinkley, J
Singh, RP
AF Pandey, Gajendra
Kareliya, Chirag
Hinkley, Jeffrey
Singh, Raman P.
TI Interfacial Micromechanics and Effect of Moisture on Fluorinated Epoxy
Carbon Fiber Composites
SO POLYMER COMPOSITES
LA English
DT Article
ID ADHESION; RESIN; STRENGTH; TESTS; WATER
AB Carbon fiber composites have witnessed an increased application in aerospace and other civil structures due to their excellent structural properties such as specific strength and stiffness. However, unlike other structural materials, carbon fiber composites have not been as widely studied. Hence, their increased application is also accompanied with a serious concern about their long-term durability. Many of these applications are exposed to multiple environments such as moisture, temperature, and UV radiation. Composites based on conventional epoxies readily absorb moisture. However, recently synthesized fluorinated epoxies show reduced moisture absorption and hence potentially better long-term durability. The aim of this project is to study the effect of moisture absorption on fluorinated-epoxy-based carbon fiber composites and their comparison with conventional epoxy carbon fiber-based composites. Microbond tests are performed on fluorinated and nonfluorinated epoxy-based single fiber samples before and after boiling water degradation. It is found that fluorinated epoxy-based single fiber coupons showed relatively reduced degradation of interface when compared with the nonfluorinated epoxy single fiber coupons. POLYM. COMPOS., 32:1961-1969, 2011. (C) 2011 Society of Plastics Engineers
C1 [Pandey, Gajendra; Kareliya, Chirag; Singh, Raman P.] Oklahoma State Univ, Helmerich Res Ctr, Sch Mech & Aerosp Engn, Mech Adv Mat Lab, Tulsa, OK 74106 USA.
[Hinkley, Jeffrey] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Singh, RP (reprint author), Oklahoma State Univ, Helmerich Res Ctr, Sch Mech & Aerosp Engn, Mech Adv Mat Lab, 526 N Elgin Ave, Tulsa, OK 74106 USA.
EM raman.singh@okstate.edu
FU NASA EPSCoR; Oklahoma NASA EPSCoR office
FX Contract grant sponsors: NASA EPSCoR program and Oklahoma NASA EPSCoR
office.
NR 40
TC 7
Z9 7
U1 3
U2 21
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0272-8397
EI 1548-0569
J9 POLYM COMPOSITE
JI Polym. Compos.
PD DEC
PY 2011
VL 32
IS 12
BP 1961
EP 1969
DI 10.1002/pc.21227
PG 9
WC Materials Science, Composites; Polymer Science
SC Materials Science; Polymer Science
GA 854SS
UT WOS:000297515300007
ER
PT J
AU Yang, H
Magpayo, N
Rusek, A
Chiang, IH
Sivertz, M
Held, KD
AF Yang, H.
Magpayo, N.
Rusek, A.
Chiang, I-H.
Sivertz, M.
Held, K. D.
TI Effects of Very Low Fluences of High-Energy Protons or Iron Ions on
Irradiated and Bystander Cells
SO RADIATION RESEARCH
LA English
DT Article
ID DOUBLE-STRAND BREAKS; MEDIATED INTERCELLULAR COMMUNICATION; HUMAN
FIBROBLASTS; ALPHA-PARTICLES; IN-VIVO; RADIATION ONCOGENESIS;
IONIZING-RADIATION; MICRONUCLEUS ASSAY; GAMMA-IRRADIATION; SPACE
EXPLORATION
AB Yang, H., Magpayo, N., Rusek, A., Chiang, I-H., Sivertz, M. and Held, K. D. Effects of Very Low Fluences of High-Energy Protons or Iron Ions on Irradiated and Bystander Cells. Radiat. Res. 176, 695-705 (2011).
In space, astronauts are exposed to radiation fields consisting of energetic protons and high atomic number, high-energy (HZE) particles at very low dose rates or fluences. Under these conditions, it is likely that, in addition to cells in an astronaut's body being traversed by ionizing radiation particles, unirradiated cells can also receive intercellular bystander signals from irradiated cells. Thus this study was designed to determine the dependence of DNA damage induction on dose at very low fluences of charged particles. Novel techniques to quantify particle fluence have been developed at the NASA Space Radiation Biology Laboratory (NSRL) at Brookhaven National Laboratory (BNL). The approach uses a large ionization chamber to visualize the radiation beam coupled with a scintillation counter to measure fluence. This development has allowed us to irradiate cells with 1 GeV/nucleon protons and iron ions at particle fluences as low as 200 particles/cm(2) and quantify biological responses. Our results show an increased fraction of cells with DNA damage in both the irradiated population and bystander cells sharing medium with irradiated cells after low fluences. The fraction of cells with damage, manifest as micronucleus formation and 53BP1 focus induction, is about 2-fold higher than background at doses as low as similar to 0.47 mGy iron ions (similar to 0.02 iron ions/cell) or similar to 70 mu Gy protons (similar to 2 protons/cell). In the irradiated population, irrespective of radiation type, the fraction of damaged cells is constant from the lowest damaging fluence to about 1 cGy, above which the fraction of damaged cells increases with dose. In the bystander population, the level of damage is the same as in the irradiated population up to 1 cGy, but it does not increase above that plateau level with increasing dose. The data suggest that at fluences of high-energy protons or iron ions less than about 5 cGy, the response in irradiated cell populations may be dominated by the bystander response. (C) 2011 by Radiation Research Society
C1 [Yang, H.; Magpayo, N.; Held, K. D.] Harvard Univ, Dept Radiat Oncol, Massachusetts Gen Hosp, Sch Med,COX 302, Boston, MA 02114 USA.
[Rusek, A.; Chiang, I-H.; Sivertz, M.] NASA, Space Radiat Biol Lab, Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Held, KD (reprint author), Harvard Univ, Dept Radiat Oncol, Massachusetts Gen Hosp, Sch Med,COX 302, 55 Fruit St, Boston, MA 02114 USA.
EM kheld@partners.org
FU NASA [NNX07AE40G]
FX The authors acknowledge the excellent assistance from the support
personnel in the Medical and Biology Departments of Brookhaven National
Laboratory. The authors thank Drs. Kevin M. Prise, Howard L. Liber and
Robert W. Redmond for many helpful discussions. This research was
supported by NASA grant no. NNX07AE40G.
NR 56
TC 15
Z9 15
U1 1
U2 6
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
J9 RADIAT RES
JI Radiat. Res.
PD DEC
PY 2011
VL 176
IS 6
BP 695
EP 705
DI 10.1667/RR2674.1
PG 11
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA 859VN
UT WOS:000297904000001
PM 21988573
ER
PT J
AU Slaba, TC
Blattnig, SR
Clowdsley, MS
AF Slaba, Tony C.
Blattnig, Steve R.
Clowdsley, Martha S.
TI Variation in Lunar Neutron Dose Estimates
SO RADIATION RESEARCH
LA English
DT Article
ID RADIATION PROTECTION DOSIMETRY; GALACTIC COSMIC-RAYS; MAN ANATOMICAL
MODEL; ADULT VOXEL PHANTOM; CONVERSION COEFFICIENTS; MONOENERGETIC
NEUTRONS; FLUENCE; ENVIRONMENT; CODE; EXPLORATION
AB Slaba, T. C., Blattnig, S. R. and Clowdsley, M. S., Variation in Lunar Neutron Dose Estimates. Radiat. Res. 176, 827-841 (2011).
The radiation environment on the Moon includes albedo neutrons produced by primary particles interacting with the lunar surface. In this work, HZETRN2010 is used to calculate the albedo neutron contribution to effective dose as a function of shielding thickness for four different space radiation environments and to determine to what extent various factors affect such estimates. First, albedo neutron spectra computed with HZETRN2010 are compared to Monte Carlo results in various radiation environments. Next, the impact of lunar regolith composition on the albedo neutron spectrum is examined, and the variation on effective dose caused by neutron fluent e-to-effective dose conversion coefficients is studied. A methodology for computing effective dose in detailed human phantoms using HZETRN2010 is also discussed and compared. Finally, the combined variation caused by environmental models, shielding materials, shielding thickness, regolith composition and conversion coefficients on the albedo neutron contribution to effective dose is determined. It is shown that a single percentage number for characterizing the albedo neutron contribution to effective dose can be misleading. In general, the albedo neutron contribution to effective dose is found to vary between 1-32%, with the environmental model, shielding material and shielding thickness being the driving factors that determine the exact contribution. It is also shown that polyethylene or other hydrogen-rich materials may be used to mitigate the albedo neutron exposure. (C) 2011 by Radiation Research Society
C1 [Slaba, Tony C.; Blattnig, Steve R.; Clowdsley, Martha S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Slaba, TC (reprint author), NASA, Langley Res Ctr, 2 W Reid St,MS 188E, Hampton, VA 23681 USA.
EM Tony.C.Slaba@nasa.gov
FU Advanced Capabilities Division under Exploration Systems Mission
Directorate of NASA
FX This work was supported by the Human Research Program in the Advanced
Capabilities Division under the Exploration Systems Mission Directorate
of NASA.
NR 49
TC 6
Z9 6
U1 0
U2 4
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
J9 RADIAT RES
JI Radiat. Res.
PD DEC
PY 2011
VL 176
IS 6
BP 827
EP 841
DI 10.1667/RR2616.1
PG 15
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA 859VN
UT WOS:000297904000016
PM 21859325
ER
PT J
AU Aliu, E
Aune, T
Beilicke, M
Benbow, W
Bottcher, M
Bouvier, A
Bradbury, SM
Buckley, JH
Bugaev, V
Cannon, A
Cesarini, A
Ciupik, L
Connolly, MP
Cui, W
Decerprit, G
Dickherber, R
Duke, C
Errando, M
Falcone, A
Feng, Q
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Hivick, B
Holder, J
Huan, H
Hughes, G
Hui, CM
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Krawczynski, H
Krennrich, F
Maier, G
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Nelson, T
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pichel, A
Pohl, M
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Ruppel, J
Saxon, DB
Sembroski, GH
Skole, C
Smith, AW
Staszak, D
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Tyler, J
Varlotta, A
Vassiliev, VV
Wakely, SP
Weekes, TC
Weinstein, A
Williams, DA
Zitzer, B
Ciprini, S
Fumagalli, M
Kaplan, K
Paneque, D
Prochaska, JX
AF Aliu, E.
Aune, T.
Beilicke, M.
Benbow, W.
Boettcher, M.
Bouvier, A.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Cannon, A.
Cesarini, A.
Ciupik, L.
Connolly, M. P.
Cui, W.
Decerprit, G.
Dickherber, R.
Duke, C.
Errando, M.
Falcone, A.
Feng, Q.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Godambe, S.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Hivick, B.
Holder, J.
Huan, H.
Hughes, G.
Hui, C. M.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Nelson, T.
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pichel, A.
Pohl, M.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Ruppel, J.
Saxon, D. B.
Sembroski, G. H.
Skole, C.
Smith, A. W.
Staszak, D.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Wakely, S. P.
Weekes, T. C.
Weinstein, A.
Williams, D. A.
Zitzer, B.
Ciprini, S.
Fumagalli, M.
Kaplan, K.
Paneque, D.
Prochaska, J. X.
CA VERITAS Collaboration
TI MULTIWAVELENGTH OBSERVATIONS OF THE PREVIOUSLY UNIDENTIFIED BLAZAR RX
J0648.7+1516
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (RX J0648.7+1516, 1FGL J0648.8+1516, VER
J0648+152); gamma rays: galaxies
ID LARGE-AREA TELESCOPE; BL-LACERTAE OBJECTS; ALL-SKY SURVEY;
PARTICLE-ACCELERATION; SOURCE CATALOG; RAY; VERITAS; MISSION
AB We report on the VERITAS discovery of very high energy (VHE) gamma-ray emission above 200 GeV from the high-frequency-peaked BL Lac (HBL) object RX J0648.7+1516 (GB J0648+1516), associated with 1FGL J0648.8+1516. The photon spectrum above 200 GeV is fitted by a power law dN/dE = F-0(E/E-0)(-Gamma) with a photon index Gamma of 4.4 +/- 0.8(stat) +/- 0.3(syst) and a flux normalization F-0 of (2.3 +/- 0.5(stat) +/- 1.2(sys)) x 10(-11) TeV-1 cm(-2) s(-1) with E-0 = 300 GeV. No VHE variability is detected during VERITAS observations of RX J0648.7+1516 between 2010 March 4 and April 15. Following the VHE discovery, the optical identification and spectroscopic redshift were obtained using the Shane 3 m Telescope at the Lick Observatory, showing the unidentified object to be a BL Lac type with a redshift of z = 0.179. Broadband multiwavelength observations contemporaneous with the VERITAS exposure period can be used to subclassify the blazar as an HBL object, including data from the MDM observatory, Swift-UVOT, and X-Ray Telescope, and continuous monitoring at photon energies above 1 GeV from the Fermi Large Area Telescope (LAT). We find that in the absence of undetected, high-energy rapid variability, the one-zone synchrotron self-Compton (SSC) model overproduces the high-energy gamma-ray emission measured by the Fermi-LAT over 2.3 years. The spectral energy distribution can be parameterized satisfactorily with an external-Compton or lepto-hadronic model, which have two and six additional free parameters, respectively, compared to the one-zone SSC model.
C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Bouvier, A.; 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.
[Benbow, W.; Galante, N.; Roache, E.; Theiling, M.; Weekes, T. C.; Kaplan, K.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Boettcher, M.; Hivick, B.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Cannon, A.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Connolly, M. P.; Gillanders, G. H.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Feng, Q.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Decerprit, G.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Skole, C.] DESY, D-15738 Zeuthen, Germany.
[Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[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.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Holder, J.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; Humensky, T. B.; Park, N.; Reyes, L. C.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Perkins, J. S.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Pohl, M.; Ruppel, J.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Ciprini, S.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Fumagalli, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Prochaska, J. X.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
EM afurniss@ucsc.edu; miki@ucolick.org; dpaneque@mppmu.mpg.de
RI Fumagalli, Michele/K-9510-2015;
OI Fumagalli, Michele/0000-0001-6676-3842; Cui, Wei/0000-0002-6324-5772;
Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794
FU US Department of Energy; NSERC in Canada; Science Foundation Ireland
(SFI ) [10/RFP/AST2748]; STFC in the UK; NASA [NNX10AF89G]; Fermi
[NNX09AU18G]; NSF [AST-0548180]; US National Science Foundation;
Smithsonian Institution
FX VERITAS is supported by the US Department of Energy, US National Science
Foundation, and Smithsonian Institution, by NSERC in Canada, by Science
Foundation Ireland (SFI 10/RFP/AST2748), and STFC in the UK. We
acknowledge the excellent work of the technical support staff at the
FLWO and at the collaborating institutions. This work was also supported
by NASA grants from the Swift (NNX10AF89G) and Fermi (NNX09AU18G) Guest
Investigator programs.; J.X.P. acknowledges funding through an NSF
CAREER grant (AST-0548180).
NR 33
TC 22
Z9 23
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 DEC 1
PY 2011
VL 742
IS 2
AR 127
DI 10.1088/0004-637X/742/2/127
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900067
ER
PT J
AU Assef, RJ
Denney, KD
Kochanek, CS
Peterson, BM
Kozeowski, S
Ageorges, N
Barrows, RS
Buschkamp, P
Dietrich, M
Falco, E
Feiz, C
Gemperlein, H
Germeroth, A
Grier, CJ
Hofmann, R
Juette, M
Khan, R
Kilic, M
Knierim, V
Laun, W
Lederer, R
Lehmitz, M
Lenzen, R
Mall, U
Madsen, KK
Mandel, H
Martini, P
Mathur, S
Mogren, K
Mueller, P
Naranjo, V
Pasquali, A
Polsterer, K
Pogge, RW
Quirrenbach, A
Seifert, W
Stern, D
Shappee, B
Storz, C
Van Saders, J
Weiser, P
Zhang, D
AF Assef, R. J.
Denney, K. D.
Kochanek, C. S.
Peterson, B. M.
Kozeowski, S.
Ageorges, N.
Barrows, R. S.
Buschkamp, P.
Dietrich, M.
Falco, E.
Feiz, C.
Gemperlein, H.
Germeroth, A.
Grier, C. J.
Hofmann, R.
Juette, M.
Khan, R.
Kilic, M.
Knierim, V.
Laun, W.
Lederer, R.
Lehmitz, M.
Lenzen, R.
Mall, U.
Madsen, K. K.
Mandel, H.
Martini, P.
Mathur, S.
Mogren, K.
Mueller, P.
Naranjo, V.
Pasquali, A.
Polsterer, K.
Pogge, R. W.
Quirrenbach, A.
Seifert, W.
Stern, D.
Shappee, B.
Storz, C.
Van Saders, J.
Weiser, P.
Zhang, D.
TI BLACK HOLE MASS ESTIMATES BASED ON CIV ARE CONSISTENT WITH THOSE BASED
ON THE BALMER LINES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; gravitational lensing: strong; quasars: emission lines
ID ACTIVE GALACTIC NUCLEI; NEAR-INFRARED SPECTROSCOPY; QUASI-STELLAR
OBJECTS; EARLY-TYPE GALAXIES; DIGITAL-SKY-SURVEY; EMISSION-LINE; BROAD
EMISSION; HIGH-REDSHIFT; GRAVITATIONAL LENSES; VELOCITY DISPERSION
AB Using a sample of high-redshift lensed quasars from the CASTLES project with observed-frame ultraviolet or optical and near-infrared spectra, we have searched for possible biases between supermassive black hole (BH) mass estimates based on the C IV, H alpha, and H beta broad emission lines. Our sample is based upon that of Greene, Peng, & Ludwig, expanded with new near-IR spectroscopic observations, consistently analyzed high signal-to-noise ratio (S/N) optical spectra, and consistent continuum luminosity estimates at 5100 angstrom. We find that BH mass estimates based on the full width at half-maximum (FWHM) of C IV show a systematic offset with respect to those obtained from the line dispersion, sigma(l), of the same emission line, but not with those obtained from the FWHM of H alpha and H beta. The magnitude of the offset depends on the treatment of the He II and Fe II emission blended with C IV, but there is little scatter for any fixed measurement prescription. While we otherwise find no systematic offsets between C IV and Balmer line mass estimates, we do find that the residuals between them are strongly correlated with the ratio of the UV and optical continuum luminosities. This means that much of the dispersion in previous comparisons of C IV and H beta BH mass estimates are due to the continuum luminosities rather than to any properties of the lines. Removing this dependency reduces the scatter between the UV- and optical-based BH mass estimates by a factor of approximately two, from roughly 0.35 to 0.18 dex. The dispersion is smallest when comparing the C IV sigma(l) mass estimate, after removing the offset from the FWHM estimates, and either Balmer line mass estimate. The correlation with the continuum slope is likely due to a combination of reddening, host contamination, and object-dependent SED shapes. When we add additional heterogeneous measurements from the literature, the results are unchanged. Moreover, in a trial observation of a remaining outlier, the origin of the deviation is clearly due to unrecognized absorption in a low S/N spectrum. This not only highlights the importance of the quality of the observations, but also raises the question whether cases like this one are common in the literature, further biasing comparisons between C IV and other broad emission lines.
C1 [Assef, R. J.; Denney, K. D.; Kochanek, C. S.; Peterson, B. M.; Kozeowski, S.; Dietrich, M.; Grier, C. J.; Khan, R.; Martini, P.; Mathur, S.; Mogren, K.; Pogge, R. W.; Shappee, B.; Van Saders, J.; Zhang, D.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Assef, R. J.; Denney, K. D.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Kochanek, C. S.; Peterson, B. M.; Martini, P.; Mathur, S.; Pogge, R. W.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Ageorges, N.; Buschkamp, P.; Gemperlein, H.; Hofmann, R.; Lederer, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Barrows, R. S.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA.
[Falco, E.; Kilic, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Feiz, C.; Germeroth, A.; Mandel, H.; Mueller, P.; Quirrenbach, A.] Heidelberg Univ, ZAH, D-69117 Heidelberg, Germany.
[Juette, M.; Knierim, V.; Polsterer, K.] Astron Inst Ruhr Univ, D-44780 Bochum, Germany.
[Laun, W.; Lehmitz, M.; Lenzen, R.; Mall, U.; Naranjo, V.; Pasquali, A.; Storz, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Madsen, K. K.] CALTECH, Pasadena, CA 91125 USA.
[Weiser, P.] Fachhsch Tech & Gestaltung, D-68163 Mannheim, Germany.
RP Assef, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
EM rjassef@astronomy.ohio-state.edu
RI Peterson, Bradley/G-8226-2012; Kozlowski, Szymon/G-4799-2013; Khan,
Rubab/F-9455-2015
OI Kozlowski, Szymon/0000-0003-4084-880X; Khan, Rubab/0000-0001-5100-5168
FU NASA at the Jet Propulsion Laboratory; NASA; NSF [AST-0708082,
AST-1009756, AST-1008882, AST-0705170]
FX We thank Jenny E. Greene, Christopher Onken, Chien Y. Peng, Kristen
Sellgren, Marianne Vestergaard, and Linda Watson for their help and
suggestions that improved our work. We thank F. Courbin, E. Mediavilla,
V. Motta, L. J. Goicoechea, S. Sluse, J. L. Tonry, L. Wisotzki, and J.
Munoz for sending us their optical spectra of Q2237+030, SDSS1138+0314,
Q0957+561, HE1104-1805, B1422+231, and SBS0909+532. We thank F. Harrison
for helping us obtain an optical spectrum of SDSS1151+0340. We also
thank all the people in the LUCIFER science demonstration time team who
did not participate directly in this work. We thank the anonymous
referee for suggestions that helped improve our work. R. J. A. was
supported in part by an appointment to the NASA Postdoctoral Program at
the Jet Propulsion Laboratory, administered by Oak Ridge Associated
Universities through a contract with NASA. C. S. K. is supported by NSF
grants AST-0708082 and AST-1009756. B. M. P., M. D., and R. W. P. are
supported by NSF grant AST-1008882. P. M. is supported by NSF grant
AST-0705170. 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 101
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U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
AR 93
DI 10.1088/0004-637X/742/2/93
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900033
ER
PT J
AU Coyner, AJ
Davila, JM
AF Coyner, Aaron J.
Davila, Joseph M.
TI DETERMINATION OF NON-THERMAL VELOCITY DISTRIBUTIONS FROM SERTS LINEWIDTH
OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: UV radiation
ID EXTREME-ULTRAVIOLET SPECTRA; EUV IMAGING SPECTROMETER; EMISSION-LINE
PROFILES; SOLAR ACTIVE-REGION; ATOMIC DATABASE; ALFVEN WAVES; CORONA;
CHROMOSPHERE; WIDTHS; LIMB
AB Non-thermal velocities obtained from the measurement of coronal Extreme Ultraviolet (EUV) linewidths have been consistently observed in solar EUV spectral observations and have been theorized to result from many plausible scenarios including wave motions, turbulence, or magnetic reconnection. Constraining these velocities can provide a physical limit for the available energy resulting from unresolved motions in the corona. We statistically determine a series of non-thermal velocity distributions from linewidth measurements of 390 emission lines from a wide array of elements and ionization states observed during the Solar Extreme Ultraviolet Research Telescope and Spectrograph 1991-1997 flights covering the spectral range 174-418 angstrom and a temperature range from 80,000 K to 12.6 MK. This sample includes 248 lines from active regions, 101 lines from quiet-Sun regions, and 41 lines were observed from plasma off the solar limb. We find a strongly peaked distribution corresponding to a non-thermal velocity of 19-22 km s(-1) in all three of the quiet-Sun, active region, and off-limb distributions. For the possibility of Alfven wave resonance heating, we find that velocities in the core of these distributions do not provide sufficient energy, given typical densities and magnetic field strengths for the coronal plasma, to overcome the estimated coronal energy losses required to maintain the corona at the typical temperatures working as the sole mechanism. We find that at perfect efficiency 50%-60% of the needed energy flux can be produced from the non-thermal velocities measured.
C1 [Coyner, Aaron J.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Coyner, Aaron J.; Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Coyner, AJ (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave, Washington, DC 20064 USA.
EM aaron.j.coyner@nasa.gov
NR 28
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U1 2
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
AR 115
DI 10.1088/0004-637X/742/2/115
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900055
ER
PT J
AU Finkelstein, KD
Papovich, C
Finkelstein, SL
Willmer, CNA
Rigby, JR
Rudnick, G
Egami, E
Rieke, M
Smith, JDT
AF Finkelstein, Keely D.
Papovich, Casey
Finkelstein, Steven L.
Willmer, Christopher N. A.
Rigby, Jane R.
Rudnick, Gregory
Egami, Eiichi
Rieke, Marcia
Smith, J. -D. T.
TI PROBING THE STAR FORMATION HISTORY AND INITIAL MASS FUNCTION OF THE z
similar to 2.5 LENSED GALAXY SMM J163554.2+661225 WITH HERSCHEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; galaxies: individual (SMM J163554.2+661225);
galaxies: starburst; infrared: galaxies
ID SPECTRAL ENERGY-DISTRIBUTION; SPITZER-SPACE-TELESCOPE; INFRARED
GALAXIES; FORMING GALAXIES; CONFUSION LIMIT; HUBBLE SEQUENCE; DUST;
EMISSION; SPIRE; LUMINOSITY
AB We present the analysis of Herschel Spectral and Photometric Imaging Receiver far-infrared (FIR) observations of the z = 2.515 lensed galaxy SMM J163554.2+661225. Combining new 250, 350, and 500 mu m observations with existing data, we make an improved fit to the FIR spectral energy distribution of this galaxy. We find a total infrared (IR) luminosity of L(8-1000 mu m) = 6.9 +/- 0.6 x 10(11) L-circle dot, a factor of three more precise over previous L-IR estimates for this galaxy, and one of the most accurate measurements for any galaxy at these redshifts. This FIR luminosity implies an unlensed star formation rate (SFR) for this galaxy of 119 +/- 10 M-circle dot yr(-1), which is a factor of 1.9 +/- 0.35 lower than the SFR derived from the nebular Pa alpha emission line (a 2.5 sigma discrepancy). Both SFR indicators assume an identical Salpeter initial mass function (IMF) with slope Gamma = 2.35 over a mass range of 0.1-100 M-circle dot; thus this discrepancy suggests that more ionizing photons may be necessary to account for the higher Pa alpha-derived SFR. We examine a number of scenarios and find that the observations can be explained with a varying star formation history (SFH) due to an increasing SFR, paired with a slight flattening of the IMF. If the SFR is constant in time, then larger changes need to be made to the IMF by either increasing the upper mass cutoff to similar to 200 M-circle dot, or a flattening of the IMF slope to 1.9 +/- 0.15, or a combination of the two. These scenarios result in up to double the number of stars with masses above 20 M-circle dot, which produce the requisite increase in ionizing photons over a Salpeter IMF with a constant SFH.
C1 [Finkelstein, Keely D.; Papovich, Casey; Finkelstein, Steven L.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Finkelstein, Keely D.; Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Finkelstein, Keely D.; Finkelstein, Steven L.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Willmer, Christopher N. A.; Egami, Eiichi; Rieke, Marcia] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rudnick, Gregory] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Smith, J. -D. T.] Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA.
RP Finkelstein, KD (reprint author), Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU NASA [HST-HF-51288.01, NAS 5-26555]; Texas AM University; Space
Telescope Science Institute
FX The authors wish to thank Kim-Vy Tran for many useful conversations,
Jean-Paul Kneib for his help on questions regarding the lensing model,
as well as Rob Ivison and Anthony Smith for help with questions
regarding the HerMES survey. We also thank the anonymous referee for a
very useful report which improved the quality of this paper. This
research has made use of data from HerMES project (Oliver et al. 2010;
http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme
utilizing Guaranteed Time from the SPIRE instrument team, ESAC
scientists, and a mission scientist. The HerMES data were accessed
through the HeDaM database (http://hedam.oamp.fr) operated by CeSAM and
hosted by the Laboratoire d'Astrophysique de Marseille. This work is
based in part on observations made with the Herschel Space Observatory
and 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. Further support for K. D. F., C. P., and S. L. F. was
provided by Texas A&M University. S. L. F. also received support by NASA
through Hubble Fellowship Grant HST-HF-51288.01, awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555.
NR 63
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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 DEC 1
PY 2011
VL 742
IS 2
AR 108
DI 10.1088/0004-637X/742/2/108
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900048
ER
PT J
AU Gou, LJ
McClintock, JE
Reid, MJ
Orosz, JA
Steiner, JF
Narayan, R
Xiang, JG
Remillard, RA
Arnaud, KA
Davis, SW
AF Gou, Lijun
McClintock, Jeffrey E.
Reid, Mark J.
Orosz, Jerome A.
Steiner, James F.
Narayan, Ramesh
Xiang, Jingen
Remillard, Ronald A.
Arnaud, Keith A.
Davis, Shane W.
TI THE EXTREME SPIN OF THE BLACK HOLE IN CYGNUS X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; stars: individual
(Cygnus X-1); X-rays: binaries
ID X-RAY BINARIES; CONTINUUM-FITTING METHOD; ACCRETION DISK MODELS; DWARF
NOVA OUTBURSTS; EMISSION-LINES; INNER-DISK; SOFT STATE; LMC X-1; MASS;
REFLECTION
AB The compact primary in the X-ray binary Cygnus X-1 was the first black hole to be established via dynamical observations. We have recently determined accurate values for its mass and distance, and for the orbital inclination angle of the binary. Building on these results, which are based on our favored (asynchronous) dynamical model, we have measured the radius of the inner edge of the black hole's accretion disk by fitting its thermal continuum spectrum to a fully relativistic model of a thin accretion disk. Assuming that the spin axis of the black hole is aligned with the orbital angular momentum vector, we have determined that Cygnus X-1 contains a near-extreme Kerr black hole with a spin parameter a(*) > 0.95 (3 sigma). For a less probable (synchronous) dynamical model, we find a(*) > 0.92 (3 sigma). In our analysis, we include the uncertainties in black hole mass, orbital inclination angle, and distance, and we also include the uncertainty in the calibration of the absolute flux via the Crab. These four sources of uncertainty totally dominate the error budget. The uncertainties introduced by the thin-disk model we employ are particularly small in this case given the extreme spin of the black hole and the disk's low luminosity.
C1 [Gou, Lijun; McClintock, Jeffrey E.; Reid, Mark J.; Steiner, James F.; Narayan, Ramesh; Xiang, Jingen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Arnaud, Keith A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Arnaud, Keith A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Davis, Shane W.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
RP Gou, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Narayan, Ramesh/0000-0002-1919-2730
FU NASA [DD0-11049X, DD1-12054X, NNX11AD08G]; Smithsonian Endowment Funds
FX We thank an anonymous referee for very helpful and constructive
comments. We are grateful to Director H. Tanananbaum and Project
Scientist T. Strohmayer for granting us, respectively, Chandra and RXTE
observing time. We thank H. Marshall, M. Nowak, and N. Schulz for help
in planning the Chandra observations, and M. Hanke, M. Nowak, and J.
Wilms for discussions on X-ray data analysis. The research has made use
of data obtained from the High Energy Astrophysics Science Archive
Research Center (HEASARC) at NASA/Goddard Space Flight Center. L. G.
thanks the Harvard FAS Sciences Division Research Computing Group for
their technical support on the Odyssey cluster. J. E. M. acknowledges
support from NASA grants DD0-11049X, DD1-12054X, and NNX11AD08G, and the
Smithsonian Endowment Funds.
NR 80
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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 DEC 1
PY 2011
VL 742
IS 2
AR 85
DI 10.1088/0004-637X/742/2/85
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900025
ER
PT J
AU Jiang, C
Jiang, BW
Christensen-Dalsgaard, J
Bedding, TR
Stello, D
Huber, D
Frandsen, S
Kjeldsen, H
Karoff, C
Mosser, B
Demarque, P
Fanelli, MN
Kinemuchi, K
Mullally, F
AF Jiang, C.
Jiang, B. W.
Christensen-Dalsgaard, J.
Bedding, T. R.
Stello, D.
Huber, D.
Frandsen, S.
Kjeldsen, H.
Karoff, C.
Mosser, B.
Demarque, P.
Fanelli, M. N.
Kinemuchi, K.
Mullally, F.
TI MODELING KEPLER OBSERVATIONS OF SOLAR-LIKE OSCILLATIONS IN THE RED GIANT
STAR HD 186355
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; stars: fundamental parameters; stars: individual
(HD 186355); stars: oscillations; stars: solar-type
ID MAIN-SEQUENCE STARS; 1ST 4 MONTHS; EPSILON-OPHIUCHI; STELLAR
OSCILLATIONS; GRAVITY MODES; K-GIANTS; ASTEROSEISMOLOGY; PARAMETERS;
PHOTOMETRY; COROT
AB We have analyzed oscillations of the red giant star HD 186355 observed by the NASA Kepler satellite. The data consist of the first five quarters of science operations of Kepler, which cover about 13 months. The high-precision time-series data allow us to accurately extract the oscillation frequencies from the power spectrum. We find that the frequency of the maximum oscillation power, nu(max), and the mean large frequency separation, Delta nu, are around 106 and 9.4 mu Hz, respectively. A regular pattern of radial and non-radial oscillation modes is identified by stacking the power spectra in an echelle diagram. We use the scaling relations of Delta nu and nu(max) to estimate the preliminary asteroseismic mass, which is confirmed with the modeling result (M = 1.45 +/- 0.05 M-circle dot) using the Yale Rotating stellar Evolution Code (YREC7). In addition, we constrain the effective temperature, luminosity, and radius from comparisons between observational constraints and models. A number of mixed l = 1 modes are also detected and taken into account in our model comparisons. We find a mean observational period spacing for these mixed modes of about 58 s, suggesting that this red giant branch star is in the shell hydrogen-burning phase.
C1 [Jiang, C.; Jiang, B. W.] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China.
[Christensen-Dalsgaard, J.; Frandsen, S.; Kjeldsen, H.; Karoff, C.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Bedding, T. R.; Stello, D.; Huber, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Mosser, B.] Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Demarque, P.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Fanelli, M. N.; Kinemuchi, K.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Mullally, F.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Jiang, C (reprint author), Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China.
EM jiangchen@mail.bnu.edu.cn
OI Bedding, Timothy/0000-0001-5943-1460; Karoff,
Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661
FU NASA's Science Mission Directorate; China's NSFC [10973004]; China 973
Program [2007CB815406]; Fundamental Research Funds for the Central
Universities
FX The authors acknowledge the Kepler Science Team for their work to
provide us with these great data. Funding for the Kepler Discovery
mission is provided by NASA's Science Mission Directorate. This work is
supported by China's NSFC through the project 10973004, China 973
Program 2007CB815406, and the Fundamental Research Funds for the Central
Universities.
NR 63
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Z9 16
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
AR 120
DI 10.1088/0004-637X/742/2/120
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900060
ER
PT J
AU Lotz, JM
Jonsson, P
Cox, TJ
Croton, D
Primack, JR
Somerville, RS
Stewart, K
AF Lotz, Jennifer M.
Jonsson, Patrik
Cox, T. J.
Croton, Darren
Primack, Joel R.
Somerville, Rachel S.
Stewart, Kyle
TI THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: interactions;
galaxies: structure
ID STAR-FORMING GALAXIES; HIGH-REDSHIFT GALAXIES; DARK-MATTER HALOES; VLT
DEEP SURVEY; SIMILAR-TO 1; SUPERMASSIVE BLACK-HOLES; MASS ASSEMBLY
HISTORIES; ACTIVE GALACTIC NUCLEI; EXTENDED GROTH STRIP; DIGITAL SKY
SURVEY
AB Calculating the galaxy merger rate requires both a census of galaxies identified as merger candidates and a cosmologically averaged "observability" timescale < T-obs(z)> for identifying galaxy mergers. While many have counted galaxy mergers using a variety of techniques, < T-obs(z)> for these techniques have been poorly constrained. We address this problem by calibrating three merger rate estimators with a suite of hydrodynamic merger simulations and three galaxy formation models. We estimate < T-obs(z)> for (1) close galaxy pairs with a range of projected separations, (2) the morphology indicator G - M-20, and (3) the morphology indicator asymmetry Lambda A. Then, we apply these timescales to the observed merger fractions at z < 1.5 from the recent literature. When our physically motivated timescales are adopted, the observed galaxy merger rates become largely consistent. The remaining differences between the galaxy merger rates are explained by the differences in the ranges of the mass ratio measured by different techniques and differing parent galaxy selection. The major merger rate per unit comoving volume for samples selected with constant number density evolves much more strongly with redshift (alpha (1 + z)(+3.0 +/- 1.1)) than samples selected with constant stellar mass or passively evolving luminosity (alpha (1 + z)(+0.1 +/- 0.4)). We calculate the minor merger rate (1:4 < M-sat/M-primary less than or similar to 1:10) by subtracting the major merger rate from close pairs from the "total" merger rate determined by G - M-20. The implied minor merger rate is similar to 3 times the major merger rate at z similar to 0.7 and shows little evolution with redshift.
C1 [Lotz, Jennifer M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Lotz, Jennifer M.; Somerville, Rachel S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cox, T. J.] Carnegie Observ, Pasadena, CA USA.
[Croton, Darren] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Somerville, Rachel S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Stewart, Kyle] Jet Prop Lab, Pasadena, CA USA.
RP Lotz, JM (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA.
EM lotz@stsci.edu
FU NOAO; W. M. Keck Foundation; Australian Government; Office of Science of
the U.S. Department of Energy
FX We thank L. Lin, L. de Ravel, J. Kartaltepe, and Y. Shi for sending us
detailed versions of their data and calculations. We thank N. Scoville,
K. Bundy, P. Hopkins, and the anonymous referee for helpful comments on
earlier version of this manuscript. We acknowledge the use of S. Salim's
measurements of the stellar masses for galaxies in the Extended Groth
Strip. J. M. L. acknowledges support from the NOAO Leo Goldberg
Fellowship. P. J. was supported by a grant from the W. M. Keck
Foundation. D. C. acknowledges receipt of a QEII Fellowship by the
Australian Government. This research used computational resources of the
NASA Advanced Supercomputing Division (NAS) and the National Energy
Research Scientific Computing Center (NERSC), which is supported by the
Office of Science of the U.S. Department of Energy.
NR 122
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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 DEC 1
PY 2011
VL 742
IS 2
DI 10.1088/0004-637X/742/2/103
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900043
ER
PT J
AU Miller, KA
Smith, WW
Ehrenreich, T
Kessel, QC
Pollack, E
Verzani, C
Kharchenko, VA
Chutjian, A
Lozano, JA
Djuric, N
Smith, SJ
AF Miller, K. A.
Smith, W. W.
Ehrenreich, T.
Kessel, Q. C.
Pollack, E.
Verzani, C.
Kharchenko, V. A.
Chutjian, A.
Lozano, J. A.
Djuric, N.
Smith, S. J.
TI X-RAY EMISSIONS FROM COLLISIONS OF O6+ IONS WITH CO
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; molecular processes; solar wind
ID SELECTIVE ELECTRON-CAPTURE; CHARGE-EXCHANGE EMISSION; SOLAR-WIND IONS;
LI-LIKE IONS; CROSS-SECTIONS; SLOW COLLISIONS; COMETS; CHANDRA; ATOMS;
SPECTRA
AB Laboratory measurements of soft X-ray emissions from collisions between 36 keV O6+ ions and CO have been carried out with the aim of simulating emissions from comets interacting with the solar wind. Spectra in the range 62-155 eV are recorded and compared to results of the over-barrier model (OBM) and multichannel Landau-Zener (MLZ) calculations. Emissions from n = 3, 4 states of O5+ are observed. This is in good agreement with the OBM predictions of highest n-state for the electron capture. Line intensities for the n = 4 capture in simulated spectra using the semi-empirical MLZ approach, taking into account multielectron captures, are in very good agreement with experimental measurements. However, the OBM does not correctly account for direct feeding of the n = 3 levels for the CO target, though it does explain predominance of the n = 3 levels for an He target.
C1 [Miller, K. A.; Smith, W. W.; Ehrenreich, T.; Kessel, Q. C.; Pollack, E.; Verzani, C.; Kharchenko, V. A.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Chutjian, A.; Lozano, J. A.; Djuric, N.; Smith, S. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Miller, KA (reprint author), Columbia Univ, Astrophys Lab, New York, NY 10027 USA.
FU National Aeronautics and Space Administration (NASA) [NCC5-601]; Caltech
FX We acknowledge the seminal contribution of the late Professor Edward
Pollack in initiating this collaboration with JPL and in writing the
original UConn NASA grant proposal. Helpful discussions with E. Seder,
A. Wrigley, and W. Gohn are also acknowledged. Work at the University of
Connecticut was supported by NASA Grant NCC5-601. Work at JPL/Caltech
was supported through agreement between Caltech and the National
Aeronautics and Space Administration.
NR 44
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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 DEC 1
PY 2011
VL 742
IS 2
AR 130
DI 10.1088/0004-637X/742/2/130
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900070
ER
PT J
AU Reardon, KP
Wang, YM
Muglach, K
Warren, HP
AF Reardon, K. P.
Wang, Y. -M.
Muglach, K.
Warren, H. P.
TI EVIDENCE FOR TWO SEPARATE BUT INTERLACED COMPONENTS OF THE CHROMOSPHERIC
MAGNETIC FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: chromosphere; Sun: corona; Sun: faculae, plages; Sun: magnetic
topology; Sun: surface magnetism
ID SOLAR CHROMOSPHERE; HIGH-RESOLUTION; DYNAMIC FIBRILS; ACTIVE REGIONS;
FINE-STRUCTURE; IBIS; NETWORK; CORONA; EVOLUTION; SPICULES
AB Chromospheric fibrils are generally thought to trace out low-lying, mainly horizontal magnetic fields that fan out from flux concentrations in the photosphere. A high-resolution (similar to 0 ''.1 pixel(-1)) image, taken in the core of the Ca II 854.2 nm line and covering an unusually large area, shows the dark fibrils within an active region remnant as fine, looplike features that are aligned parallel to each other and have lengths comparable to a supergranular diameter. Comparison with simultaneous line-of-sight magnetograms confirms that the fibrils are centered above intranetwork areas (supergranular cell interiors), with one end rooted just inside the neighboring plage or strong unipolar network but the other endpoint less clearly defined. Focusing on a particular arcade-like structure lying entirely on one side of a filament channel (large-scale polarity inversion), we find that the total amount of positive-polarity flux underlying this "fibril arcade" is similar to 50 times greater than the total amount of negative-polarity flux. Thus, if the fibrils represent closed loops, they must consist of very weak fields (in terms of total magnetic flux), which are interpenetrated by a more vertical field that contains most of the flux. This surprising result suggests that the fibrils in unipolar regions connect the network to the nearby intranetwork flux, while the bulk of the network flux links to remote regions of the opposite polarity, forming a second, higher canopy above the fibril canopy. The chromospheric field near the edge of the network thus has an interlaced structure resembling that in sunspot penumbrae.
C1 [Reardon, K. P.] Osserv Astrofis Arcetri, I-50125 Florence, Italy.
[Wang, Y. -M.; Warren, H. P.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Muglach, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reardon, K. P.] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Muglach, K.] ARTEP Inc, Ellicott City, MD 21042 USA.
RP Reardon, KP (reprint author), Osserv Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.
EM kreardon@arcetri.astro.it; yi.wang@nrl.navy.mil; karin.muglach@nasa.gov;
hwarren@nrl.navy.mil
FU NASA; NSF; ONR
FX We thank G. Cauzzi and N.R. Sheeley, Jr. for stimulating discussions,
the referee for helpful comments, and the AIA and HMI science teams for
providing the SDO data. IBIS was built by INAF/OAA with contributions
from the University of Florence, University of Rome, MIUR, and MAE, and
is operated with the support of NSO. This work was funded by NASA, NSF,
and ONR.
NR 26
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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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
AR 119
DI 10.1088/0004-637X/742/2/119
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900059
ER
PT J
AU Ruhlen, L
Smith, DM
Swank, JH
AF Ruhlen, L.
Smith, D. M.
Swank, J. H.
TI THE NATURE AND CAUSE OF SPECTRAL VARIABILITY IN LMC X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: winds, outflows; X-rays: binaries
ID X-RAY BINARIES; BLACK-HOLE BINARY; RADIATION-DRIVEN WINDS; CYGNUS X-1;
ACCRETION DISK; SOFT STATE; HDE 226868; HOT STARS; MASS; MODEL
AB We present the results of a long-term observation campaign of the extragalactic wind-accreting black hole X-ray binary LMC X-1, using the Proportional Counter Array on RXTE. The observations show that LMC X-1's accretion disk exhibits an anomalous temperature-luminosity relation. We use deep archival RXTE observations to show that large movements across the temperature-luminosity space occupied by the system can take place on timescales as short as half an hour. These changes cannot be adequately explained by perturbations that propagate from the outer disk on a viscous timescale. We propose instead that the apparent disk variations reflect rapid fluctuations within the Compton upscattering coronal material, which occults the inner parts of the disk. The expected relationship between the observed disk luminosity and apparent disk temperature derived from the variable occultation model is quantitatively shown to be in good agreement with the observations. Two other observations support this picture: an inverse correlation between the flux in the power-law spectral component and the fitted inner-disk temperature, and a near-constant total photon flux, suggesting that the inner disk is not ejected when a lower temperature is observed.
C1 [Ruhlen, L.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
[Smith, D. M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Swank, J. H.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Ruhlen, L (reprint author), Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
EM lruhlen@ucsc.edu; dsmith@scipp.ucsc.edu; swank@lheavx.gsfc.nasa.gov
RI Swank, Jean/F-2693-2012
FU NASA [NNX09AC86G]
FX This work was supported by NASA grant NNX09AC86G. The authors thank the
anonymous referee for constructive and insightful suggestions. L. R.
thanks E. Ramirez-Ruiz, R. Strickler, and J. Naiman for productive
discussions.
NR 53
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U2 4
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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 DEC 1
PY 2011
VL 742
IS 2
AR 75
DI 10.1088/0004-637X/742/2/75
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900015
ER
PT J
AU Teng, SH
Mushotzky, RF
Sambruna, RM
Davis, DS
Reynolds, CS
AF Teng, Stacy H.
Mushotzky, Richard F.
Sambruna, Rita M.
Davis, David S.
Reynolds, Christopher S.
TI FERMI/LAT OBSERVATIONS OF SWIFT/BAT SEYFERT GALAXIES: ON THE
CONTRIBUTION OF RADIO-QUIET ACTIVE GALACTIC NUCLEI TO THE EXTRAGALACTIC
gamma-RAY BACKGROUND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; gamma rays: diffuse background;
X-rays: diffuse background; X-rays: galaxies
ID ADVECTION-DOMINATED ACCRETION; BURST ALERT TELESCOPE; LARGE-AREA
TELESCOPE; BLAZAR SEQUENCE; BLACK-HOLES; SKY SURVEY; LUMINOSITY;
EMISSION; CATALOG; ORIGIN
AB We present the analysis of 2.1 years of Fermi Large Area Telescope (LAT) data on 491 Seyfert galaxies detected by the Swift Burst Alert Telescope (BAT) survey. Only the two nearest objects, NGC 1068 and NGC 4945, which were identified in the Fermi first year catalog, are detected. Using Swift/BAT and radio 20 cm fluxes, we define a new radio-loudness parameter R-X,R-BAT where radio-loud objects have log R-X,R-BAT > -4.7. Based on this parameter, only radio-loud sources are detected by Fermi/LAT. An upper limit to the flux of the undetected sources is derived to be similar to 2x10(-11) photons cm(-2) s(-1), approximately seven times lower than the observed flux of NGC 1068. Assuming a median redshift of 0.031, this implies an upper limit to the gamma-ray (1-100 GeV) luminosity of less than or similar to 3 x 10(41) erg s(-1). In addition, we identified 120 newFermi/LAT sources near the Swift/BAT Seyfert galaxies with significant Fermi/LAT detections. A majority of these objects do not have Swift/BAT counterparts, but their possible optical counterparts include blazars, flat-spectrum radio quasars, and quasars.
C1 [Teng, Stacy H.; Mushotzky, Richard F.; Reynolds, Christopher S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Teng, Stacy H.; Davis, David S.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
[Teng, Stacy H.; Davis, David S.] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Sambruna, Rita M.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
[Davis, David S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RP Teng, SH (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM stacyt@astro.umd.edu
FU NASA
FX We are grateful to the referee for providing insightful comments that
improved the manuscript. We thank Wayne Baumgartner and the Swift/BAT
team for providing the BAT 58 month catalog ahead of its release. We
made use of the NASA/IPAC Extragalactic Databased (NED), which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. We acknowledge support by NASA
through the Fermi General Observer Program.
NR 32
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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 DEC 1
PY 2011
VL 742
IS 2
AR 66
DI 10.1088/0004-637X/742/2/66
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900006
ER
PT J
AU van der Wel, A
Straughn, AN
Rix, HW
Finkelstein, SL
Koekemoer, AM
Weiner, BJ
Wuyts, S
Bell, EF
Faber, SM
Trump, JR
Koo, DC
Ferguson, HC
Scarlata, C
Hathi, NP
Dunlop, JS
Newman, JA
Dickinson, M
Jahnke, K
Salmon, BW
de Mello, DF
Kocevski, DD
Lai, K
Grogin, NA
Rodney, SA
Guo, YC
McGrath, EJ
Lee, KS
Barro, G
Huang, KH
Riess, AG
Ashby, MLN
Willner, SP
AF van der Wel, A.
Straughn, A. N.
Rix, H. -W.
Finkelstein, S. L.
Koekemoer, A. M.
Weiner, B. J.
Wuyts, S.
Bell, E. F.
Faber, S. M.
Trump, J. R.
Koo, D. C.
Ferguson, H. C.
Scarlata, C.
Hathi, N. P.
Dunlop, J. S.
Newman, J. A.
Dickinson, M.
Jahnke, K.
Salmon, B. W.
de Mello, D. F.
Kocevski, D. D.
Lai, K.
Grogin, N. A.
Rodney, S. A.
Guo, Yicheng
McGrath, E. J.
Lee, K. -S.
Barro, G.
Huang, K. -H.
Riess, A. G.
Ashby, M. L. N.
Willner, S. P.
TI EXTREME EMISSION-LINE GALAXIES IN CANDELS: BROADBAND-SELECTED,
STARBURSTING DWARF GALAXIES AT z > 1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies:
high-redshift; galaxies: starburst
ID EARLY RELEASE SCIENCE; LY-ALPHA EMITTERS; ORIGINS DEEP SURVEY; GREEN PEA
GALAXIES; STAR-FORMATION; FORMATION HISTORIES; MASS FUNCTION; LOCAL
VOLUME; FIELD; EVOLUTION
AB We identify an abundant population of extreme emission-line galaxies (EELGs) at redshift z similar to 1.7 in the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey imaging from Hubble Space Telescope/Wide Field Camera 3 (HST/WFC3). Sixty-nine EELG candidates are selected by the large contribution of exceptionally bright emission lines to their near-infrared broadband magnitudes. Supported by spectroscopic confirmation of strong [OIII] emission lines-with rest-frame equivalent widths similar to 1000 angstrom-in the four candidates that have HST/WFC3 grism observations, we conclude that these objects are galaxies with similar to 10(8) M-circle dot in stellar mass, undergoing an enormous starburst phase with M-*/(M) over dot(*) of only similar to 15 Myr. These bursts may cause outflows that are strong enough to produce cored dark matter profiles in low-mass galaxies. The individual star formation rates and the comoving number density (3.7 x 10(-4) Mpc(-3)) can produce in similar to 4 Gyr much of the stellar mass density that is presently contained in 10(8)-10(9) M-circle dot dwarf galaxies. Therefore, our observations provide a strong indication that many or even most of the stars in present-day dwarf galaxies formed in strong, short-lived bursts, mostly at z > 1.
C1 [van der Wel, A.; Rix, H. -W.; Jahnke, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Straughn, A. N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Finkelstein, S. L.; Salmon, B. W.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Koekemoer, A. M.; Ferguson, H. C.; Grogin, N. A.; Riess, A. G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Weiner, B. J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Wuyts, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Faber, S. M.; Trump, J. R.; Koo, D. C.; Kocevski, D. D.; Lai, K.; McGrath, E. J.; Barro, G.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Scarlata, C.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Hathi, N. P.] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
[Dunlop, J. S.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Newman, J. A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Dickinson, M.] Natl Optic Astron Observ, Tucson, AZ 85719 USA.
[de Mello, D. F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[de Mello, D. F.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Rodney, S. A.; Huang, K. -H.; Riess, A. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Guo, Yicheng] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Lee, K. -S.] Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.
[Ashby, M. L. N.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP van der Wel, A (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM vdwel@mpia.de
RI Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Koekemoer, Anton/0000-0002-6610-2048;
Bell, Eric/0000-0002-5564-9873
FU HST [GO-12060]; NSF [AST 08-08133]
FX A.v.d.W. thanks the following people for useful feedback and stimulating
discussions: Greg Stinson, Andrea Maccio, Brent Groves, Dan Weisz, Joe
Hennawi, Kate Rubin, Sharon Meidt, and Marijn Franx. S.M.F., J.R.T.,
D.C.K., D.D.K., K.L., and E.G.M. acknowledge funding through HST
GO-12060 and NSF AST 08-08133.
NR 64
TC 69
Z9 69
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 DEC 1
PY 2011
VL 742
IS 2
AR 111
DI 10.1088/0004-637X/742/2/111
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900051
ER
PT J
AU Zitrin, A
Broadhurst, T
Coe, D
Umetsu, K
Postman, M
Benitez, N
Meneghetti, M
Medezinski, E
Jouvel, S
Bradley, L
Koekemoer, A
Zheng, W
Ford, H
Merten, J
Kelson, D
Lahav, O
Lemze, D
Molino, A
Nonino, M
Donahue, M
Rosati, P
Van der Wel, A
Bartelmann, M
Bouwens, R
Graur, O
Graves, G
Host, O
Infante, L
Jha, S
Jimenez-Teja, Y
Lazkoz, R
Maoz, D
McCully, C
Melchior, P
Moustakas, LA
Ogaz, S
Patel, B
Regoes, E
Riess, A
Rodney, S
Seitz, S
AF Zitrin, A.
Broadhurst, T.
Coe, D.
Umetsu, K.
Postman, M.
Benitez, N.
Meneghetti, M.
Medezinski, E.
Jouvel, S.
Bradley, L.
Koekemoer, A.
Zheng, W.
Ford, H.
Merten, J.
Kelson, D.
Lahav, O.
Lemze, D.
Molino, A.
Nonino, M.
Donahue, M.
Rosati, P.
Van der Wel, A.
Bartelmann, M.
Bouwens, R.
Graur, O.
Graves, G.
Host, O.
Infante, L.
Jha, S.
Jimenez-Teja, Y.
Lazkoz, R.
Maoz, D.
McCully, C.
Melchior, P.
Moustakas, L. A.
Ogaz, S.
Patel, B.
Regoes, E.
Riess, A.
Rodney, S.
Seitz, S.
TI THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE (CLASH):
STRONG-LENSING ANALYSIS OF A383 FROM 16-BAND HST/WFC3/ACS IMAGING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: clusters: general; galaxies: clusters:
individual: A383; galaxies: high-redshift; gravitational lensing: strong
ID PHOTOMETRIC REDSHIFT ESTIMATION; LUMINOUS GALAXY CLUSTERS; DARK-MATTER
DISTRIBUTION; DEEP ADVANCED CAMERA; X-RAY; MARENOSTRUM UNIVERSE; MASS
PROFILE; COSMOLOGICAL CONSTRAINTS; NONPARAMETRIC INVERSION; ACS/NIC3
OBSERVATIONS
AB We examine the inner mass distribution of the relaxed galaxy cluster A383 (z = 0.189), in deep 16 band Hubble Space Telescope/ACS+WFC3 imaging taken as part of the Cluster Lensing And Supernova survey with Hubble (CLASH) multi-cycle treasury program. Our program is designed to study the dark matter distribution in 25 massive clusters, and balances depth with a wide wavelength coverage, 2000-16000 angstrom, to better identify lensed systems and generate precise photometric redshifts. This photometric information together with the predictive strength of our strong-lensing analysis method identifies 13 new multiply lensed images and candidates, so that a total of 27 multiple images of nine systems are used to tightly constrain the inner mass profile gradient, d log Sigma/d log r similar or equal to -0.6 +/- 0.1 (r < 160 kpc). We find consistency with the standard distance-redshift relation for the full range spanned by the lensed images, 1.01 < z < 6.03, with the higher-redshift sources deflected through larger angles as expected. The inner mass profile derived here is consistent with the results of our independent weak-lensing analysis of wide-field Subaru images, with good agreement in the region of overlap (similar to 0.7-1 arcmin). Combining weak and strong lensing, the overall mass profile is well fitted by a Navarro-Frenk-White profile with M-vir = (5.37(-0.63)(+0.70) +/- 0.26) x 10(14) M-circle dot h(-1) and a relatively high concentration, c(vir) = 8.77(-0.42)(+0.44) +/- 0.23, which lies above the standard c-M relation similar to other well-studied clusters. The critical radius of A383 is modest by the standards of other lensing clusters, r(E) similar or equal to 16 +/- 2 '' (for z(s) = 2.55), so the relatively large number of lensed images uncovered here with precise photometric redshifts validates our imaging strategy for the CLASH survey. In total we aim to provide similarly high-quality lensing data for 25 clusters, 20 of which are X-ray-selected relaxed clusters, enabling a precise determination of the representative mass profile free from lensing bias.
C1 [Zitrin, A.; Graur, O.; Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Broadhurst, T.; Lazkoz, R.] Univ Basque Country, Dept Theoret Phys, Bilbao, Spain.
[Broadhurst, T.] Basque Fdn Sci, IKERBASQUE, Madrid, Spain.
[Coe, D.; Postman, M.; Bradley, L.; Koekemoer, A.; Ogaz, S.; Riess, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Benitez, N.; Molino, A.; Jimenez-Teja, Y.] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
[Meneghetti, M.] INAF, Osservatorio Astron Bologna, Bologna, Italy.
[Medezinski, E.; Zheng, W.; Ford, H.; Lemze, D.; Riess, A.; Rodney, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Jouvel, S.; Lahav, O.; Host, O.] UCL, Dept Phys & Astron, London, England.
[Merten, J.; Bartelmann, M.] Heidelberg Univ, Inst Theoret Astrophys, ZAH, Heidelberg, Germany.
[Kelson, D.] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
[Nonino, M.] INAF, Osservatorio Astron Trieste, Trieste, Italy.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Rosati, P.] European So Observ, D-8046 Garching, Germany.
[Van der Wel, A.] MPIA, Heidelberg, Germany.
[Bouwens, R.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Graves, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Infante, L.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile.
[Jha, S.; McCully, C.; Patel, B.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ USA.
[Melchior, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Regoes, E.] CERN, European Lab Particle Phys, CH-1211 Geneva, Switzerland.
[Seitz, S.] Univ Sternwarte Munchen, Munich, Germany.
RP Zitrin, A (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
EM adiz@wise.tau.ac.il
RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014;
Lazkoz, Ruth/A-5642-2011; Jimenez-Teja, Yolanda/D-5933-2011; Meneghetti,
Massimo/O-8139-2015;
OI Benitez, Narciso/0000-0002-0403-7455; Koekemoer,
Anton/0000-0002-6610-2048; Lazkoz, Ruth/0000-0001-5536-3130; Meneghetti,
Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Graur,
Or/0000-0002-4391-6137; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas,
Leonidas/0000-0003-3030-2360
FU NASA [HSTGO12065.01-A, NAS 5-26555]; Israel Science Foundation;
Baden-Wuerttemberg Foundation; German Science Foundation [Transregio TR
33]; Spanish MICINN [YA2010-22111-C03-00]; Junta de Andalucia Proyecto
de Excelencia [NBL2003]; INAF [ASI-INAF I/009/10/0, ASI-INAF I/023/05/0,
ASI-INAF I/088/06/0, PRIN INAF 2009, PRIN INAF 2010]; NSF [AST-0847157];
UK's STFC; Royal Society; Wolfson Foundation; DFG; National Science
Council of Taiwan [NSC97-2112-M-001-020-MY3]; John Bahcall excellence
prize
FX We thank the anonymous referee of this paper for useful comments that
improved the manuscript. The CLASH Multi-Cycle Treasury Program
(GO-12065) is based on observations made with the NASA/ESA Hubble Space
Telescope. We are especially grateful to our program coordinator Beth
Perrillo for her expert assistance in implementing the HST observations
in this program. We thank Jay Anderson and Norman Grogin for providing
the ACS CTE and bias striping correction algorithms used in our data
pipeline. We are grateful to Stefan Gottlober and Gustavo Yepes for
giving us access to the MARENOSTRUM UNIVERSE simulation and to Stefano
Ettori for helpful discussions. This research is supported in part by
NASA grant HSTGO12065.01-A, the Israel Science Foundation, the
Baden-Wuerttemberg Foundation, the German Science Foundation (Transregio
TR 33), Spanish MICINN grant YA2010-22111-C03-00, funding from the Junta
de Andalucia Proyecto de Excelencia NBL2003, INAF contracts ASI-INAF
I/009/10/0, ASI-INAF I/023/05/0, ASI-INAF I/088/06/0, PRIN INAF 2009,
and PRIN INAF 2010, NSF CAREER grant AST-0847157, the UK's STFC, the
Royal Society, the Wolfson Foundation, the DFG cluster of excellence
Origin and Structure of the Universe, and National Science Council of
Taiwan grant NSC97-2112-M-001-020-MY3. Part of this work is based on
data collected at the Subaru Telescope, which is operated by the
National Astronomical Society of Japan. A.Z. acknowledges support from
the John Bahcall excellence prize. The HST science operations center,
the Space Telescope Science Institute, is operated by the Association of
Universities for Research in Astronomy, Inc. under NASA contract NAS
5-26555.
NR 91
TC 48
Z9 48
U1 1
U2 11
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 DEC 1
PY 2011
VL 742
IS 2
AR 117
DI 10.1088/0004-637X/742/2/117
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900057
ER
PT J
AU Vrieling, A
de Beurs, KM
Brown, ME
AF Vrieling, Anton
de Beurs, Kirsten M.
Brown, Molly E.
TI Variability of African farming systems from phenological analysis of
NDVI time series
SO CLIMATIC CHANGE
LA English
DT Article
ID NET PRIMARY PRODUCTIVITY; GLOBAL LAND-COVER; TERRESTRIAL PRIMARY
PRODUCTION; SUB-SAHARAN AFRICA; CLIMATE-CHANGE; FOOD SECURITY;
EAST-AFRICA; INTERANNUAL VARIABILITY; NOAA-AVHRR; MONITORING VEGETATION
AB Food security exists when people have access to sufficient, safe and nutritious food at all times to meet their dietary needs. The natural resource base is one of the many factors affecting food security. Its variability and decline creates problems for local food production. In this study we characterize for sub-Saharan Africa vegetation phenology and assess variability and trends of phenological indicators based on NDVI time series from 1982 to 2006. We focus on cumulated NDVI over the season (cumNDVI) which is a proxy for net primary productivity. Results are aggregated at the level of major farming systems, while determining also spatial variability within farming systems. High temporal variability of cumNDVI occurs in semiarid and subhumid regions. The results show a large area of positive cumNDVI trends between Senegal and South Sudan. These correspond to positive CRU rainfall trends found and relate to recovery after the 1980's droughts. We find significant negative cumNDVI trends near the south-coast of West Africa (Guinea coast) and in Tanzania. For each farming system, causes of change and variability are discussed based on available literature (Appendix A). Although food security comprises more than the local natural resource base, our results can perform an input for food security analysis by identifying zones of high variability or downward trends. Farming systems are found to be a useful level of analysis. Diversity and trends found within farming system boundaries underline that farming systems are dynamic.
C1 [Vrieling, Anton] Univ Twente, Fac Geoinformat Sci & Earth Observat ITC, NL-7500 AE Enschede, Netherlands.
[de Beurs, Kirsten M.] Univ Oklahoma, Dept Geog, Norman, OK 73019 USA.
[Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Vrieling, A (reprint author), Univ Twente, Fac Geoinformat Sci & Earth Observat ITC, POB 217, NL-7500 AE Enschede, Netherlands.
EM a.vrieling@utwente.nl
RI Vrieling, Anton/B-2639-2012; Faculty of ITC, Dep Nat.
Resources/C-4295-2014; Brown, Molly/M-5146-2013; Brown,
Molly/E-2724-2010
OI Vrieling, Anton/0000-0002-7979-1540; Brown, Molly/0000-0001-7384-3314;
Brown, Molly/0000-0001-7384-3314
NR 103
TC 33
Z9 34
U1 3
U2 31
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
J9 CLIMATIC CHANGE
JI Clim. Change
PD DEC
PY 2011
VL 109
IS 3-4
BP 455
EP 477
DI 10.1007/s10584-011-0049-1
PG 23
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 852IH
UT WOS:000297350700013
ER
PT J
AU Freedman, WL
Madore, BF
Scowcroft, V
Monson, A
Persson, SE
Seibert, M
Rigby, JR
Sturch, L
Stetson, P
AF Freedman, Wendy L.
Madore, Barry F.
Scowcroft, Victoria
Monson, Andy
Persson, S. E.
Seibert, Mark
Rigby, Jane R.
Sturch, Laura
Stetson, Peter
TI THE CARNEGIE HUBBLE PROGRAM
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE distance scale; galaxies: distances and redshifts; stars: variables:
Cepheids
ID PERIOD-LUMINOSITY RELATION; LARGE-MAGELLANIC-CLOUD; INTERSTELLAR
EXTINCTION LAW; SPITZER-SPACE-TELESCOPE; PROBE WMAP OBSERVATIONS; RED
GIANT BRANCH; 8.0 MU-M; LEAVITT LAW; DISTANCE SCALE; IA SUPERNOVAE
AB We present an overview of and preliminary results from an ongoing comprehensive program that has a goal of determining the Hubble constant to a systematic accuracy of +/- 2%. As part of this program, we are currently obtaining 3.6 mu m data using the Infrared Array Camera on Spitzer, and the program is designed to include James Webb Space Telescope in the future. We demonstrate that the mid-infrared period-luminosity relation for Cepheids at 3.6 mu m is the most accurate means of measuring Cepheid distances to date. At 3.6 mu m, it is possible to minimize the known remaining systematic uncertainties in the Cepheid extragalactic distance scale. We discuss the advantages of 3.6 mu m observations in minimizing systematic effects in the Cepheid calibration of H(0) including the absolute zero point, extinction corrections, and the effects of metallicity on the colors and magnitudes of Cepheids. We undertake three independent tests of the sensitivity of the mid-IR Cepheid Leavitt Law to metallicity, which when combined will allow a robust constraint on the effect. Finally, we provide a new mid-IR Tully-Fisher relation for spiral galaxies.
C1 [Freedman, Wendy L.; Madore, Barry F.; Scowcroft, Victoria; Monson, Andy; Persson, S. E.; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Rigby, Jane R.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sturch, Laura] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Stetson, Peter] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada.
RP Freedman, WL (reprint author), Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
EM wendy@obs.carnegiescience.edu; barry@obs.carnegiescience.edu;
vs@obs.carnegiescience.edu; amonson@obs.carnegiescience.edu;
persson@obs.carnegiescience.edu; mseibert@obs.carnegiescience.edu;
Jane.R.Rigby@nasa.gov; lsturch@bu.edu; Peter.Stetson@nrc-cnrc.gc.ca
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU NASA; NASA through JPL/Caltech
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 by NASA through an award issued by
JPL/Caltech. We thank the staff of the Spitzer Science Center for their
help with the analysis of these data.
NR 48
TC 26
Z9 26
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD DEC
PY 2011
VL 142
IS 6
AR 192
DI 10.1088/0004-6256/142/6/192
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 851FT
UT WOS:000297254500014
ER
PT J
AU Jaeger, TR
Osten, RA
Lazio, TJ
Kassim, N
Mutel, RL
AF Jaeger, T. R.
Osten, R. A.
Lazio, T. J.
Kassim, N.
Mutel, R. L.
TI 325 MHz VERY LARGE ARRAY OBSERVATIONS OF ULTRACOOL DWARFS TVLM 513-46546
AND 2MASS J0036+1821104
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE brown dwarfs; radio continuum: stars; radiation mechanisms: non-thermal;
stars: activity; stars: low-mass; stars: magnetic field
ID CYCLOTRON MASER EMISSION; RADIO-EMISSION; BROWN DWARFS; X-RAY;
ROTATIONAL MODULATION; SOLAR CORONA; STARS; TVLM-513-46546; FLARE;
VARIABILITY
AB We present 325 MHz (90 cm wavelength) radio observations of ultracool dwarfs TVLM 513-46546 and 2MASS J0036+1821104 using the Very Large Array (VLA) in 2007 June. Ultracool dwarfs are expected to be undetectable at radio frequencies, yet observations at 8.5 GHz (3.5 cm) and 4.9 GHz (6 cm) have revealed sources with >100 mu Jy quiescent radio flux and >1 mJy pulses coincident with stellar rotation. The anomalous emission is likely a combination of gyrosynchrotron and cyclotron maser processes in a long-duration, large-scale magnetic field. Since the characteristic frequency for each process scales directly with the magnetic field magnitude, emission at lower frequencies may be detectable from regions with weaker field strength. We detect no significant radio emission at 325 MHz from TVLM 513-46546 or 2MASS J0036+1821104 over multiple stellar rotations, establishing 2.5 sigma total flux limits of 795 mu Jy and 942 mu Jy, respectively. Analysis of an archival VLA 1.4 GHz observation of 2MASS J0036+1821104 from 2005 January also yields a non-detection at the level of <130 mu Jy. The combined radio observation history (0.3 GHz to 8.5 GHz) for these sources suggests a continuum emission spectrum for ultracool dwarfs that is either flat or inverted below 2-3 GHz. Further, if the cyclotron maser instability is responsible for the pulsed radio emission observed on some ultracool dwarfs, our low-frequency non-detections suggest that the active region responsible for the high-frequency bursts is confined within two stellar radii and driven by electron beams with energies less than 5 keV.
C1 [Jaeger, T. R.; Kassim, N.] USN, Res Lab, Washington, DC 20375 USA.
[Osten, R. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Lazio, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mutel, R. L.] Univ Iowa, Dept Astron, Iowa City, IA 52242 USA.
RP Jaeger, TR (reprint author), USN, Res Lab, Washington, DC 20375 USA.
EM ted.jaeger.ctr@nrl.navy.mil
FU US Naval Research Laboratory; National Aeronautics and Space
Administration
FX This paper utilizes data from VLA programs AO218 and AB1169. We thank
Bill Cotton for assistance with Obit. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. This
research was performed while the primary author held a National Research
Council Research Associateship Award a the US Naval Research Laboratory.
Basic research in radio astronomy at the Naval Research Laboratory is
supported by 6.1 base funding. 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. The
LUNAR consortium is funded by the NASA Lunar Science Institute to
investigate concepts for astrophysical observatories on the Moon.
NR 43
TC 7
Z9 7
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD DEC
PY 2011
VL 142
IS 6
AR 189
DI 10.1088/0004-6256/142/6/189
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 851FT
UT WOS:000297254500011
ER
PT J
AU Shporer, A
Jenkins, JM
Rowe, JF
Sanderfer, DT
Seader, SE
Smith, JC
Still, MD
Thompson, SE
Twicken, JD
Welsh, WF
AF Shporer, Avi
Jenkins, Jon M.
Rowe, Jason F.
Sanderfer, Dwight T.
Seader, Shawn E.
Smith, Jeffrey C.
Still, Martin D.
Thompson, Susan E.
Twicken, Joseph D.
Welsh, William F.
TI DETECTION OF KOI-13.01 USING THE PHOTOMETRIC ORBIT
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE methods: data analysis; planets and satellites: detection; stars:
individual (KOI-13)
ID LIGHT CURVES; SOPHIE VELOCIMETRY; DWARF COMPANION; KEPLER-MISSION;
BINARY STARS; PLANETS; CANDIDATES; VARIABILITY; DISCOVERY; SYSTEMS
AB We use the KOI-13 transiting star-planet system as a test case for the recently developed BEER algorithm, aimed at identifying non-transiting low-mass companions by detecting the photometric variability induced by the companion along its orbit. Such photometric variability is generated by three mechanisms: the beaming effect, tidal ellipsoidal distortion, and reflection/heating. We use data from three Kepler quarters, from the first year of the mission, while ignoring measurements within the transit and occultation, and show that the planet's ephemeris is clearly detected. We fit for the amplitude of each of the three effects and use the beaming effect amplitude to estimate the planet's minimum mass, which results in M-p sin i = 9.2 +/- 1.1 M-J (assuming the host star parameters derived by Szabo et al.). Our results show that non-transiting star-planet systems similar to KOI-13.01 can be detected in Kepler data, including a measurement of the orbital ephemeris and the planet's minimum mass. Moreover, we derive a realistic estimate of the amplitudes uncertainties, and use it to show that data obtained during the entire lifetime of the Kepler mission of 3.5 years will allow detecting non-transiting close-in low-mass companions orbiting bright stars, down to the few Jupiter mass level. Data from the Kepler Extended Mission, if funded by NASA, will further improve the detection capabilities.
C1 [Shporer, Avi] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Jenkins, Jon M.; Seader, Shawn E.; Smith, Jeffrey C.; Thompson, Susan E.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Still, Martin D.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Shporer, A (reprint author), Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
EM ashporer@lcogt.net
FU NASA's Science Mission Directorate; NASA [NNX10AG02A]
FX Kepler was competitively selected as the tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate. We warmly thank Michael Endl for useful comments. A. S.
acknowledges support from NASA Grant Number NNX10AG02A.
NR 38
TC 58
Z9 58
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD DEC
PY 2011
VL 142
IS 6
AR 195
DI 10.1088/0004-6256/142/6/195
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 851FT
UT WOS:000297254500017
ER
PT J
AU Lee, JSF
Berejikian, BA
Rust, MB
Massee, K
Wright, T
Brakensiek, K
Steltzner, S
Blankenship, HL
AF Lee, Jonathan S. F.
Berejikian, Barry A.
Rust, Michael B.
Massee, Ken
Wright, Terry
Brakensiek, Kyle
Steltzner, Scott
Blankenship, H. Lee
TI Movements of hatchery-reared lingcod released on rocky reefs in Puget
Sound
SO ENVIRONMENTAL BIOLOGY OF FISHES
LA English
DT Article
ID OPHIODON-ELONGATUS; STOCK ENHANCEMENT; COASTAL FISHERIES;
BRITISH-COLUMBIA; TAGGED LINGCOD; HOMING ROUTES; HOME RANGES; FISH; BAY;
WASHINGTON
AB Fourteen sub-adult hatchery-reared lingcod (Ophiodon elongatus) were released onto reefs in South Puget Sound, Washington, USA to evaluate their movement behavior. Acoustic telemetry revealed variation in movement among individuals that was related to body size. Larger lingcod tended to leave the release reef sooner than smaller lingcod. Four lingcod left the reefs less than 10 days after release, while three lingcod left between one and 4 months after release. Seven lingcod remained at the release reefs for the entire 5-month study, though they did make apparent short-term (< 24 h duration) excursions away from the reefs. Data suggest that the frequency and duration of excursions increase with age and size in both wild and hatchery lingcod. Movement data from these hatchery lingcod and previously published studies on wild lingcod are compared.
C1 [Lee, Jonathan S. F.; Berejikian, Barry A.; Rust, Michael B.; Massee, Ken] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Manchester Res Stn, Manchester, WA 98353 USA.
[Wright, Terry] NW Indian Fisheries Commiss, Olympia, WA 98516 USA.
[Steltzner, Scott] Squaxin Isl Tribe, Shelton, WA 98584 USA.
[Blankenship, H. Lee] NW Marine Technol, Tumwater, WA 98501 USA.
RP Lee, JSF (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Manchester Res Stn, POB 130, Manchester, WA 98353 USA.
EM jon.lee@noaa.gov
FU Science Consortium for Ocean Replenishment (SCORE)
FX The authors thank Kelly Andrews for providing acoustic telemetry data on
lingcod #83, Megan Moore for making Fig. 1, the Tacoma dive club,
including Mark LaRiviere and Dave DeGroot, for diving, and Karen
Grace-Martin for statistical advice. Tom Flagg, Mark LaRiviere, Nick
Tolimieri, Culum Brown, and two anonymous reviewers improved the
manuscript with constructive comments. JSFL was supported by funds from
the Science Consortium for Ocean Replenishment (SCORE) during part of
the data analysis and manuscript preparation. The views expressed herein
are those of the authors and do not necessarily reflect those of funding
agencies.
NR 38
TC 2
Z9 2
U1 0
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0378-1909
J9 ENVIRON BIOL FISH
JI Environ. Biol. Fishes
PD DEC
PY 2011
VL 92
IS 4
BP 437
EP 445
DI 10.1007/s10641-011-9859-2
PG 9
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 843AM
UT WOS:000296644300002
ER
PT J
AU Palm, BD
Koester, DM
Driggers, WB
Sulikowski, JA
AF Palm, Brittany D.
Koester, David M.
Driggers, William B., III
Sulikowski, James A.
TI Seasonal variation in fecundity, egg case viability, gestation, and
neonate size for little skates, Leucoraja erinacea, in the Gulf of Maine
SO ENVIRONMENTAL BIOLOGY OF FISHES
LA English
DT Article
DE Rajidae; k-selected; Reproduction; Fecundity; Oviparous
ID PREDATION; LIZARDS
AB Landings of the little skate, Leucoraja erinacea, within the territorial waters of the United States are currently regulated by a federal fishery management plan (FMP). For a FMP to be effective, thorough knowledge of a species' reproductive biology is essential. Currently, little information exists on annual fecundity, egg case viability, gestation length, and neonate total length, for the little skate in the Gulf of Maine. To study these reproductive parameters, mature skates and egg cases were housed in fiberglass tanks with an open seawater system that provided natural, seasonal fluctuations in water temperature. Egg case deposition was highest during summer months with a seasonal peak in June. Of the 324 egg cases laid by seven females (c. 46 eggs per year, per female), 74.1% were viable. Gestation lengths ranged from 22 to 54 weeks throughout the four seasons. Egg cases laid in the fall had the longest gestation times (44.9 weeks, +/- 0.13 weeks) and those laid in the spring had the shortest gestation times (24.5 weeks, +/- 0.21 weeks). Total lengths of neonates from spring oviposition were statistically the longest (10.74 +/- 0.05 cm) when compared to neonates from other seasons; however, egg viability was statistically the lowest for spring when compared seasonally.
C1 [Palm, Brittany D.; Sulikowski, James A.] Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA.
[Koester, David M.] Univ New England, Dept Anat, Coll Osteopath Med, Biddeford, ME 04005 USA.
[Driggers, William B., III] Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39568 USA.
RP Palm, BD (reprint author), Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA.
EM bpalm@une.edu
NR 18
TC 6
Z9 6
U1 0
U2 17
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0378-1909
J9 ENVIRON BIOL FISH
JI Environ. Biol. Fishes
PD DEC
PY 2011
VL 92
IS 4
BP 585
EP 589
DI 10.1007/s10641-011-9854-7
PG 5
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 843AM
UT WOS:000296644300015
ER
PT J
AU Liu, Z
Dong, DN
Lundgren, P
AF Liu, Zhen
Dong, Danan
Lundgren, Paul
TI Constraints on time-dependent volcanic source models at Long Valley
Caldera from 1996 to 2009 using InSAR and geodetic measurements
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Satellite geodesy; Transient deformation; Radar interferometry; Volcano
monitoring; Volcanic hazards and risks
ID APERTURE RADAR INTERFEROMETRY; PRINCIPAL COMPONENT ANALYSIS; SURFACE
DEFORMATION; CRUSTAL DEFORMATION; SATELLITE RADAR; MAGMA INTRUSION;
CALIFORNIA; GPS; EARTHQUAKE; GRAVITY
AB Continuous monitoring of Long Valley Caldera since the late 1970s, including data from seismic and geodetic networks has shown renewed episodic unrest with accelerated uplift separated by reduced uplift, no activity, or slow deflation. We examine the time-dependent behaviour at Long Valley Caldera from 1996 to 2009 by integrating InSAR and continuous GPS (CGPS) measurements. The ERS-1/2 radar data between 1996 and 2008 and reprocessed three-component CGPS data from the Long Valley GPS network from 1996 to 2009 were combined to invert for source geometry and volume change for the following deformation episodes: 1997-1998 uplift, 2002-2003 uplift, 2004-2007 slow subsidence, and 2007-2009 slow uplift. We employed non-linear Monte-Carlo random search approaches (random cost and simulated annealing) in our inversion and examined models including spherical and finite sources (dipping prolate spheroid). Our results show that the sources of all post-2000 events (i.e. 2002-2003, 2007-2009 uplift and 2004-2007 subsidence) locate at shallow depths of similar to 6-8 km and have nearly identical surface locations, suggesting that these events may be caused by the same source in the mid-crust, possibly a mixture of hydrothermal and partial-melt magma. All three events, 2002-2003, 2004-2007, 2007-2009, are characterized by the low total volume change: similar to 0.01, similar to-0.003, similar to 0.006 km(3), respectively, with corresponding volume change rates of similar to 0.007, similar to-0.001, similar to 0.002 km(3) yr(-1). The 1997-1998 inflationary event has a steeper source geometry and much greater volume change rate (similar to 0.03 km(3) yr(-1)) than the other events, in agreement with previous studies. This suggests it is possibly driven by magma intrusion beneath the resurgent dome from a deeper source. If we regard post-2000 events as proxies for future eruption hazard, the inferred source dynamics (e.g. mid-crustal location and subdued volume change) and accompanied decrease in earthquake activity from these post-2000 events suggest that the probability for near-term eruption is low. Our study demonstrates that CGPS, along with InSAR, provide a valuable tool for monitoring time-dependent source processes at active volcanic regions.
C1 [Liu, Zhen; Dong, Danan; Lundgren, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Liu, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM zhen.liu@jpl.nasa.gov
RI Liu, Zhen/D-8334-2017
FU National Aeronautics and Space Administration
FX We thank the European Space Agency for ERS data provided through the
WInSAR archive. We thank John Langbein for stimulating discussions.
Reviews by editor Duncan Agnew and two anonymous reviewers improved this
manuscript. 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 42
TC 14
Z9 14
U1 0
U2 8
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD DEC
PY 2011
VL 187
IS 3
BP 1283
EP 1300
DI 10.1111/j.1365-246X.2011.05214.x
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 849GT
UT WOS:000297114400017
ER
PT J
AU Walker, RT
Bergman, EA
Szeliga, W
Fielding, EJ
AF Walker, R. T.
Bergman, E. A.
Szeliga, W.
Fielding, E. J.
TI Insights into the 1968-1997 Dasht-e-Bayaz and Zirkuh earthquake
sequences, eastern Iran, from calibrated relocations, InSAR and
high-resolution satellite imagery
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Interferometry; Seismicity and tectonics; Continental neotectonics;
Continental tectonics: strike-slip and transform
ID SURFACE DEFORMATION; SOURCE PARAMETERS; ACTIVE TECTONICS; MIDDLE-EAST;
FAULT; SEISMICITY; PROVINCE; PLATEAU; REGION; TURKEY
AB The sequence of seismicity in the Dasht-e-Bayaz and Zirkuh region of northeastern Iran, which includes 11 destructive earthquakes within a period of only 30 years, forms one of the most outstanding examples of clustered large and intermediate-magnitude seismic activity in the world. We perform a multiple-event relocation analysis, with procedures to remove systematic location bias, of 169 earthquakes, most of which occurred in the period 1968-2008, to better image the distribution of seismicity within this highly active part of Iran. The geographic locations of the clustered earthquakes were calibrated by the inclusion of phase arrivals from seismic stations at short epicentral distances, and also by matching the relative locations of the three largest events in the study to their mapped surface ruptures. The two independent calibration methods provide similar results that increase our confidence in the accuracy of the distribution of relocated epicentres. These calibrated epicentres, combined with the mapping of faults from high-resolution satellite imagery, and from an InSAR-derived constraint on fault location in one case, allow us to associate individual events with specific faults, and even with specific segments of faults, to better understand the nature of the active tectonics in this region during the past four decades. Several previous assumptions about the seismicity in this region are confirmed: (1) that the 1968 August 30 M(w) 7.1 Dasht-e-Bayaz earthquake nucleated at a prominent segment boundary and left-step in the fault trace, (2) that the 1968 September 11 M(w) 5.6 aftershock occurred on the Dasht-e-Bayaz fault at the eastern end of the 1968 rupture and (3) that the 1976 November 7 M(w) 6.0 Qayen earthquake probably occurred on the E-W left-lateral Avash Fault. We show, in addition, that several significant events, including the 1968 September 1 and 4 (M(w) 6.3 and 5.5) Ferdows earthquakes, the 1979 January 16 (M(w) 6.5) and 1997 June 25 (M(w) 5.9) Boznabad events and the 1979 December 7 (M(w) 5.9) Kalat-e-Shur earthquake are likely to have ruptured previously unknown faults. Our improved description of the faulting involved in the 1968-1997 earthquake sequence highlights the importance of rupturing of conjugate left-and right-lateral faults in closely spaced events, or potentially even within a single earthquake, as was likely the case at the eastern end of the 1979 November 27 (M(w) 7.1) Khuli-Buniabad main shock. The high level of clustered seismic activity probably results from the simultaneous activity on left-and right-lateral faults, an inherently unstable arrangement that must evolve rapidly. The combination of high-resolution satellite imagery and calibrated earthquake locations is a useful tool for investigating active tectonics, even in the absence of detailed field observations.
C1 [Walker, R. T.] Univ Oxford, Dept Earth Sci, Oxford OX1 3AN, England.
[Bergman, E. A.] Univ Colorado, Dept Phys, Ctr Imaging Earths Interior, Boulder, CO 80309 USA.
[Szeliga, W.; Fielding, E. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Walker, RT (reprint author), Univ Oxford, Dept Earth Sci, S Parks Rd, Oxford OX1 3AN, England.
EM Richard.Walker@earth.ox.ac.uk
RI Walker, Richard/D-9908-2011; NCEO, COMET+`/A-3443-2013; Fielding,
Eric/A-1288-2007
OI Fielding, Eric/0000-0002-6648-8067
FU University of Birjand; University of Tehran; Geological Survey of Iran;
National Aeronautics and Space Administration; Royal Society of London;
European Space Agency [C1P.6462]
FX We thank the University of Birjand, the University of Tehran and the
Geological Survey of Iran for their support of our work in Iran and for
enabling us to visit the Dasht-e-Bayaz region on several occasions. Part
of the research described in this paper was performed at the Jet
Propulsion Laboratory, California Institute of Technology under contract
with the National Aeronautics and Space Administration. IKONOS satellite
imagery was provided by the European Space Agency through project
allocation No. C1P.6462. We also thank the NERC-funded COMET+ centre in
the UK. RTW is supported by a University Research Fellowship from the
Royal Society of London.
NR 50
TC 18
Z9 18
U1 0
U2 7
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0956-540X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD DEC
PY 2011
VL 187
IS 3
BP 1577
EP 1603
DI 10.1111/j.1365-246X.2011.05213.x
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 849GT
UT WOS:000297114400033
ER
PT J
AU Pepe, A
Ortiz, AB
Lundgren, PR
Rosen, PA
Lanari, R
AF Pepe, Antonio
Ortiz, Ana Bertran
Lundgren, Paul R.
Rosen, Paul A.
Lanari, Riccardo
TI The Stripmap-ScanSAR SBAS Approach to Fill Gaps in Stripmap Deformation
Time Series With ScanSAR Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 30th IEEE International Geoscience and Remote Sensing Symposium (IGARSS)
on Remote Sensing - Global Vision for Local Action
CY JUN 25-30, 2010
CL Honolulu, HI
SP IEEE
DE Deformation time series; differential synthetic aperture radar
interferometry (DInSAR); ScanSAR interferometry; Small BAseline Subset
(SBAS)
ID SYNTHETIC-APERTURE RADAR; DIFFERENTIAL SAR INTERFEROGRAMS; CHIRP
Z-TRANSFORM; SURFACE DEFORMATION; PERMANENT SCATTERERS; DISPLACEMENT
FIELD; EARTHS SURFACE; INTERFEROMETRY; CALIFORNIA; ALGORITHM
AB We present a simple approach to jointly exploit stripmap and ScanSAR acquisitions to generate differential synthetic aperture radar interferometry (DInSAR) time series. In particular, we extend the capability of the Small BAseline Subset (SBAS) approach to compute deformation time series from a set of stripmap images by filling possible temporal gaps in the available SAR data sequence with ScanSAR acquisitions. The starting point of our approach is the raw data focusing step, which is properly carried out to align the characteristics of the ScanSAR images to those of the stripmap ones. To achieve this task, we exploit stripmap processing codes to focus both SAR data types, the ScanSAR ones being processed on a burst-by-burst basis, accounting also for possible differences of the pulse repetition frequency with respect to that of the stripmap data. The coherent combination of the focused bursts generates phase-preserved ScanSAR images with the same output geometry and pixel spacing as the stripmap ones. This allows a straightforward implementation of the next steps of the SBAS processing chain, including the inter-ferogram generation operation. In this case, we concentrate on a selection of small baseline (SB) stripmap-stripmap multilook interferograms identified through a Delaunay triangulation, which are complemented with a set of hybrid SB stripmap-ScanSAR interferograms. This interferogram selection permits us to develop an effective phase unwrapping algorithm based on a two-step processing strategy. Finally, the whole data set of unwrapped interferograms is inverted through the SBAS technique to retrieve the final deformation time series, including both stripmap and ScanSAR data. The proposed stripmap-ScanSAR SBAS processing approach is particularly attractive because it is very easy to implement since it requires only limited modifications with respect to the conventional stripmap-based SBAS algorithm. Our approach has been applied to descending and ascending hybrid stripmap-ScanSAR data sets of Envisat/ASAR C-band acquisitions from the Big Island of Hawaii. In spite of not including any common-band azimuthal filtering, which would account for the ScanSAR burst spectral properties at the expense of the algorithm simplicity, the presented results show that we may retrieve DInSAR time series with an accuracy ranging between 5 and 10 mm, consistent with previous C-band data analyses using only stripmap data.
C1 [Pepe, Antonio; Lanari, Riccardo] Italian Natl Res Council CNR, IREA, I-80124 Naples, Italy.
[Ortiz, Ana Bertran] CALTECH, Jet Prop Lab, Radar Grp, Pasadena, CA 91109 USA.
RP Pepe, A (reprint author), Italian Natl Res Council CNR, IREA, I-80124 Naples, Italy.
EM pepe.a@irea.cnr.it; nuskab2007@gmail.com; paul.r.lundgren@jpl.nasa.gov;
paul.a.rosen@jpl.nasa.gov; lanari.r@irea.cnr.it
RI Pepe, Antonio/J-9454-2016
OI Pepe, Antonio/0000-0002-7843-3565
NR 56
TC 12
Z9 13
U1 0
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD DEC
PY 2011
VL 49
IS 12
SI SI
BP 4788
EP 4804
DI 10.1109/TGRS.2011.2167979
PN 1
PG 17
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 851OU
UT WOS:000297281500011
ER
PT J
AU Jeong, MJ
Hsu, NC
Kwiatkowska, EJ
Franz, BA
Meister, G
Salustro, CE
AF Jeong, Myeong-Jae
Hsu, N. Christina
Kwiatkowska, Ewa J.
Franz, Bryan A.
Meister, Gerhard
Salustro, Clare E.
TI Impacts of Cross-Platform Vicarious Calibration on the Deep Blue Aerosol
Retrievals for Moderate Resolution Imaging Spectroradiometer Aboard
Terra
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aerosols; calibration; remote sensing; satellite applications;
terrestrial atmosphere
ID REFLECTIVE SOLAR BANDS; POLARIZATION-SENSITIVITY; MODIS; VALIDATION;
PRODUCTS
AB The retrieval of aerosol properties from spaceborne sensors requires highly accurate and precise radiometric measurements, thus placing stringent requirements on sensor calibration and characterization. For the Terra/Moderate Resolution Imaging Spectroradiometer (MODIS), the characteristics of the detectors of certain bands, particularly band 8 [(B8); 412 nm], have changed significantly over time, leading to increased calibration uncertainty. In this paper, we explore a possibility of utilizing a cross-calibration method developed for characterizing the Terra/MODIS detectors in the ocean bands by the National Aeronautics and Space Administration Ocean Biology Processing Group to improve aerosol retrieval over bright land surfaces. We found that the Terra/MODIS B8 reflectance corrected using the cross-calibration method resulted in significant improvements for the retrieved aerosol optical thickness when compared with that from the Multi-angle Imaging Spectroradiometer, Aqua/MODIS, and the Aerosol Robotic Network. The method reported in this paper is implemented for the operational processing of the Terra/MODIS Deep Blue aerosol products.
C1 [Jeong, Myeong-Jae; Hsu, N. Christina; Salustro, Clare E.] NASA, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kwiatkowska, Ewa J.] European Space Agcy, European Space Res & Technol Ctr, Wave Interact & Propagat Sect EEP, Directorate Tech & Qual Management TEC, NL-2200 AG Noordwijk, Netherlands.
[Franz, Bryan A.; Meister, Gerhard] NASA, Ocean Biol Proc Grp, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Jeong, MJ (reprint author), Gangneung Wonju Natl Univ, Kangnung 210702, South Korea.
EM mjeong@gwnu.ac.kr; Christina.Hsu@nasa.gov; ewa.kwiatkowska@gmail.com;
bryan.a.franz@nasa.gov; gerhard.meister-1@nasa.gov;
clare.salustro@gmail.com
RI Jeong, Myeong/B-8803-2008; Meister, Gerhard/F-7159-2012; Franz,
Bryan/D-6284-2012; Hsu, N. Christina/H-3420-2013
OI Franz, Bryan/0000-0003-0293-2082;
FU National Aeronautics and Space Administration; Ocean Biology Processing
Group
FX This work was supported by a grant from the National Aeronautics and
Space Administration Earth Observing System Program, managed by Hal
Maring.; The authors would like to thank the Moderate Resolution Imaging
Spectroradiometer (MODIS) Characterization Support Team for their
invaluable efforts to characterize and calibrate MODIS sensors. The
authors would also like to thank the Ocean Biology Processing Group for
their support and the MODIS Adaptive Processing System Team for
producing and distributing the MODIS products. The authors would also
like to thank the Aerosol Robotic Network (AERONET) principal
investigators, B. Holben, and their staff for the efforts in
establishing and maintaining the AERONET sites used in this study. The
Multi-angle Imaging Spectroradiometer data used in this study were
obtained from the National Aeronautics and Space Administration Langley
Research Center Atmospheric Science Data Center.
NR 24
TC 5
Z9 5
U1 1
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD DEC
PY 2011
VL 49
IS 12
SI SI
BP 4877
EP 4888
DI 10.1109/TGRS.2011.2153205
PN 1
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 851OU
UT WOS:000297281500019
ER
PT J
AU Yang, YK
Marshak, A
Palm, SP
Varnai, T
Wiscombe, WJ
AF Yang, Yuekui
Marshak, Alexander
Palm, Stephen P.
Varnai, Tamas
Wiscombe, Warren J.
TI Cloud Impact on Surface Altimetry From a Spaceborne 532-nm Micropulse
Photon-Counting Lidar: System Modeling for Cloudy and Clear Atmospheres
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE ICESat-2; lidar altimetry; path delay; polar cloud; radiative transfer
ID GREENLAND ICE-SHEET; LASER ALTIMETER; GLAS ALTIMETRY; PART II;
ROUGHNESS; PRECISION; ACCURACY; ERRORS; LAND
AB This paper establishes a framework that simulates the behavior of a spaceborne 532-nm micropulse photon-counting lidar in cloudy and clear atmospheres in support of the ICESat-2 mission. Adopted by the current mission design, the photon-counting system will be used to obtain surface altimetry for ICESat-2. To investigate how clouds affect surface elevation retrievals, a 3-D Monte Carlo radiative transfer model is used to simulate the photon path distribution and the Poisson distribution is adopted for the number of photon returns. Since the photon-counting system only registers the time of the first arriving photon within the detector "dead time," the retrieved average surface elevation tends to bias toward higher values. This is known as the first photon bias. With the scenarios simulated here, the first photon bias for clear sky is about 6.5 cm. Clouds affect surface altimetry in two ways: 1) Cloud attenuation lowers the average number of arriving photons and hence reduces the first photon bias, and 2) cloud forward scattering increases the photon path length and makes the surface appear further away from the satellite. Compared with that for clear skies, the average surface elevation detected by the photon-counting system for cloudy skies with optical depth of 1.0 is 4.0-6.0 cm lower for the simulations conducted. The effect of surface roughness on the accuracy of elevation retrievals is also discussed.
C1 [Yang, Yuekui] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Yang, Yuekui; Marshak, Alexander; Palm, Stephen P.; Varnai, Tamas; Wiscombe, Warren J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Palm, Stephen P.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Yang, YK (reprint author), Univ Space Res Assoc, Columbia, MD 21044 USA.
EM Yuekui.Yang@nasa.gov; alexander.marshak@nasa.gov;
Stephen.p.palm@nasa.gov; tamas.varnai@nasa.gov;
warren.j.wiscombe@nasa.gov
RI Wiscombe, Warren/D-4665-2012; Marshak, Alexander/D-5671-2012; Yang,
Yuekui/B-4326-2015
OI Wiscombe, Warren/0000-0001-6844-9849;
FU National Aeronautics and Space Administration
FX This work was supported by the National Aeronautics and Space
Administration's ICESat-2 Science Definition Project.
NR 31
TC 10
Z9 12
U1 1
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD DEC
PY 2011
VL 49
IS 12
SI SI
BP 4910
EP 4919
DI 10.1109/TGRS.2011.2153860
PN 1
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 851OU
UT WOS:000297281500022
ER
PT J
AU Altamirano, D
Belloni, T
Linares, M
van der Klis, M
Wijnands, R
Curran, PA
Kalamkar, M
Stiele, H
Motta, S
Munoz-Darias, T
Casella, P
Krimm, H
AF Altamirano, D.
Belloni, T.
Linares, M.
van der Klis, M.
Wijnands, R.
Curran, P. A.
Kalamkar, M.
Stiele, H.
Motta, S.
Munoz-Darias, T.
Casella, P.
Krimm, H.
TI THE FAINT "HEARTBEATS" OF IGR J17091-3624: AN EXCEPTIONAL BLACK HOLE
CANDIDATE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: close; black hole physics; stars: individual (IGR J17091-3624,
GRS 1915+105); X-rays: binaries
ID QUASI-PERIODIC OSCILLATIONS; MICROQUASAR GRS 1915+105; PROPORTIONAL
COUNTER ARRAY; RAY-TIMING-EXPLORER; SPECTRAL STATES; GRS-1915+105;
VARIABILITY; RXTE; BINARIES; GALAXY
AB We report on the first 180 days of Rossi X-Ray Timing Explorer observations of the outburst of the black hole candidate IGR J17091-3624. This source exhibits a broad variety of complex light curve patterns including periods of strong flares alternating with quiet intervals. Similar patterns in the X-ray light curves have been seen in the (up to now) unique black hole system GRS 1915+105. In the context of the variability classes defined by Belloni et al. for GRS 1915+105, we find that IGR J17091-3624 shows the nu, rho, alpha, lambda, beta, and mu classes as well as quiet periods which resemble the chi class, all occurring at 2-60 keV count rate levels which can be 10-50 times lower than observed in GRS 1915+105. The so-called rho class "heartbeats" occur as fast as every few seconds and as slow as similar to 100 s, tracing a loop in the hardness-intensity diagram which resembles that previously seen in GRS 1915+105. However, while GRS 1915+105 traverses this loop clockwise, IGR J17091-3624 does so in the opposite sense. We briefly discuss our findings in the context of the models proposed for GRS 1915+105 and find that either all models requiring near Eddington luminosities for GRS 1915+105-like variability fail, or IGR J17091-3624 lies at a distance well in excess of 20 kpc, or it harbors one of the least massive black holes known (<3 M-circle dot).
C1 [Altamirano, D.; van der Klis, M.; Wijnands, R.; Kalamkar, M.] Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands.
[Belloni, T.; Stiele, H.; Motta, S.; Munoz-Darias, T.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Linares, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Curran, P. A.] Ctr Saclay, CEA DSM IRFU SAp, Lab AIM, F-91191 Gif Sur Yvette, France.
[Munoz-Darias, T.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Casella, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Krimm, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimm, H.] CRESST, Greenbelt, MD 20771 USA.
[Krimm, H.] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Altamirano, D (reprint author), Univ Amsterdam, Astron Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
EM d.altamirano@uva.nl
RI Curran, Peter/B-5293-2013;
OI Curran, Peter/0000-0003-3003-4626; Casella,
Piergiorgio/0000-0002-0752-3301
FU NWO; European Community [FP7/2007-2013, ITN 215212]; Spanish MEC
[CSD2006-00070]
FX We thank Dave Russell and James Miller-Jones for insightful discussions.
M. L. acknowledges support from an NWO Rubicon fellowship. The research
leading to these results has received funding from the European
Community's Seventh Framework Programme (FP7/2007-2013) under grant
agreement number ITN 215212 "Black Hole Universe," and from the Spanish
MEC under the Consolider-Ingenio 2010 Programme grant CSD2006-00070:
"First Science with the GTC."
NR 48
TC 43
Z9 43
U1 0
U2 12
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 DEC 1
PY 2011
VL 742
IS 2
AR L17
DI 10.1088/2041-8205/742/2/L17
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846SY
UT WOS:000296924700001
ER
PT J
AU Arcavi, I
Gal-Yam, A
Yaron, O
Sternberg, A
Rabinak, I
Waxman, E
Kasliwal, MM
Quimby, RM
Ofek, EO
Horesh, A
Kulkarni, SR
Filippenko, AV
Silverman, JM
Cenko, SB
Li, WD
Bloom, JS
Sullivan, M
Nugent, PE
Poznanski, D
Gorbikov, E
Fulton, BJ
Howell, DA
Bersier, D
Riou, A
Lamotte-Bailey, S
Griga, T
Cohen, JG
Hachinger, S
Polishook, D
Xu, D
Ben-Ami, S
Manulis, I
Walker, ES
Maguire, K
Pan, YC
Matheson, T
Mazzali, PA
Pian, E
Fox, DB
Gehrels, N
Law, N
James, P
Marchant, JM
Smith, RJ
Mottram, CJ
Barnsley, RM
Kandrashoff, MT
Clubb, KI
AF Arcavi, Iair
Gal-Yam, Avishay
Yaron, Ofer
Sternberg, Assaf
Rabinak, Itay
Waxman, Eli
Kasliwal, Mansi M.
Quimby, Robert M.
Ofek, Eran O.
Horesh, Assaf
Kulkarni, Shrinivas R.
Filippenko, Alexei V.
Silverman, Jeffrey M.
Cenko, S. Bradley
Li, Weidong
Bloom, Joshua S.
Sullivan, Mark
Nugent, Peter E.
Poznanski, Dovi
Gorbikov, Evgeny
Fulton, Benjamin J.
Howell, D. Andrew
Bersier, David
Riou, Amedee
Lamotte-Bailey, Stephane
Griga, Thomas
Cohen, Judith G.
Hachinger, Stephan
Polishook, David
Xu, Dong
Ben-Ami, Sagi
Manulis, Ilan
Walker, Emma S.
Maguire, Kate
Pan, Yen-Chen
Matheson, Thomas
Mazzali, Paolo A.
Pian, Elena
Fox, Derek B.
Gehrels, Neil
Law, Nicholas
James, Philip
Marchant, Jonathan M.
Smith, Robert J.
Mottram, Chris J.
Barnsley, Robert M.
Kandrashoff, Michael T.
Clubb, Kelsey I.
TI SN 2011dh: DISCOVERY OF A TYPE IIb SUPERNOVA FROM A COMPACT PROGENITOR
IN THE NEARBY GALAXY M51
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE supernovae: individual (PTF11eon/SN2011dh)
ID CORE-COLLAPSE SUPERNOVAE; SHOCK BREAKOUT; SUPERGIANT PROGENITOR;
SPECTRAL EVOLUTION; LIGHT-CURVE; EMISSION; SN-1993J; M81; CALIBRATION;
PHOTOMETRY
AB On 2011 May 31 UT a supernova (SN) exploded in the nearby galaxy M51 (the Whirlpool Galaxy). We discovered this event using small telescopes equipped with CCD cameras and also detected it with the Palomar Transient Factory survey, rapidly confirming it to be a Type II SN. Here, we present multi-color ultraviolet through infrared photometry which is used to calculate the bolometric luminosity and a series of spectra. Our early-time observations indicate that SN 2011dh resulted from the explosion of a relatively compact progenitor star. Rapid shock-breakout cooling leads to relatively low temperatures in early-time spectra, compared to explosions of red supergiant stars, as well as a rapid early light curve decline. Optical spectra of SN 2011dh are dominated by H lines out to day 10 after explosion, after which He I lines develop. This SN is likely a member of the eIIb (compact IIb) class, with progenitor radius larger than that of SN 2008ax and smaller than the eIIb (extended IIb) SN 1993J progenitor. Our data imply that the object identified in pre-explosion Hubble Space Telescope images at the SN location is possibly a companion to the progenitor or a blended source, and not the progenitor star itself, as its radius (similar to 10(13) cm) would be highly inconsistent with constraints from our post-explosion spectra.
C1 [Arcavi, Iair; Gal-Yam, Avishay; Yaron, Ofer; Sternberg, Assaf; Rabinak, Itay; Waxman, Eli; Polishook, David; Xu, Dong; Ben-Ami, Sagi; Manulis, Ilan] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Kasliwal, Mansi M.; Quimby, Robert M.; Ofek, Eran O.; Horesh, Assaf; Kulkarni, Shrinivas R.; Cohen, Judith G.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Filippenko, Alexei V.; Silverman, Jeffrey M.; Cenko, S. Bradley; Li, Weidong; Bloom, Joshua S.; Nugent, Peter E.; Poznanski, Dovi; Kandrashoff, Michael T.; Clubb, Kelsey I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Sullivan, Mark; Maguire, Kate; Pan, Yen-Chen] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England.
[Nugent, Peter E.; Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Gorbikov, Evgeny] Tel Aviv Univ, Fac Exact Sci, Wise Observ, IL-69978 Tel Aviv, Israel.
[Gorbikov, Evgeny] Tel Aviv Univ, Fac Exact Sci, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Fulton, Benjamin J.; Howell, D. Andrew] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Bersier, David; James, Philip; Marchant, Jonathan M.; Smith, Robert J.; Mottram, Chris J.; Barnsley, Robert M.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Hachinger, Stephan; Mazzali, Paolo A.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Pian, Elena] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Matheson, Thomas] Natl Opt Astron Observ, Syst Sci Ctr, Tucson, AZ 85719 USA.
[Mazzali, Paolo A.] INAF, Osservatorio Astron Padova, Padua, Italy.
[Pian, Elena] INAF, Astron Observ Trieste, I-34143 Trieste, Italy.
[Fox, Derek B.] Penn State Univ, Eberly Coll Sci, University Pk, PA 16802 USA.
[Gehrels, Neil] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Law, Nicholas] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Arcavi, I (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
EM iair.arcavi@weizmann.ac.il
RI Gehrels, Neil/D-2971-2012; WAXMAN, ELI/K-1557-2012; Horesh,
Assaf/O-9873-2016;
OI Horesh, Assaf/0000-0002-5936-1156; Sullivan, Mark/0000-0001-9053-4820;
James, Philip/0000-0003-4131-5183; Pian, Elena/0000-0001-8646-4858;
Gal-Yam, Avishay/0000-0002-3653-5598
FU Israeli Science Foundation; US-Israel Binational Science Foundation; EU;
Minerva; US Department of Energy Scientific Discovery
[DE-FG02-06ER06-04]; Royal Society; Weizmann-UK; Richard and Rhoda
Goldman Fund; US National Science Foundation [AST-0908886]; TABASGO
Foundation; NSF-CDI [0941742]; NSF/AAG [NSF/AST-100991]; INAF; Israel
Space Agency (ISA); Max Planck Institute for Astronomy (MPA) in
Heidelberg, Germany; German Israeli Science Foundation for Research and
Development; Israel Science Foundation; W.M. Keck Foundation; Harvard
University; University of Virginia; SAO, UC Berkeley; NASA [NNX09AQ66Q,
NNX10A128G]; Office of Science of the U.S. Department of Energy
[DE-AC02-05CH11231]
FX The Weizmann Institute PTF partnership is supported by the Israeli
Science Foundation via grants to A. G. Collaborative work between A. G.
and S. R. K. is supported by the US-Israel Binational Science
Foundation. A. G. further acknowledges support from the EU FP7 Marie
Curie program via an IRG fellowship and a Minerva grant. P.E.N. is
supported by the US Department of Energy Scientific Discovery through
Advanced Computing program under contract DE-FG02-06ER06-04. M. S.
acknowledges support from the Royal Society; M. S. and A. G. are also
grateful for a Weizmann-UK Making Connections grant. A.V.F.'s supernova
group at U. C. Berkeley acknowledges generous support from Gary and
Cynthia Bengier, the Richard and Rhoda Goldman Fund, US National Science
Foundation grant AST-0908886, and the TABASGO Foundation. J.S.B.
acknowledges support of an NSF-CDI grant 0941742 and NSF/AAG grant
NSF/AST-100991. P. M., E. P., and E. S. W. acknowledge financial support
from INAF through PRIN INAF 2009.; Instrumentation at Wise Observatory
was funded in part by the Israel Space Agency (ISA), the Max Planck
Institute for Astronomy (MPA) in Heidelberg, Germany, the German Israeli
Science Foundation for Research and Development, and the Israel Science
Foundation. The WHT is operated by the Isaac Newton Group in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias. The Byrne Observatory at Sedgwick (BOS) is operated by the
Las Cumbres Observatory Global Telescope Network. The W. M. Keck
Observatory is operated as a scientific partnership among the California
Institute of Technology, the University of California, and NASA; it was
made possible by the generous financial support of the W.M. Keck
Foundation. PAIRITEL is operated by the Smithsonian Astrophysical
Observatory (SAO) and supported by the Harvard University Milton Fund,
the University of Virginia, SAO, UC Berkeley, and NASA via Swift Guest
Investigator programs NNX09AQ66Q and NNX10A128G. We are grateful to the
dedicated staffs at all of the observatories where we obtained data.;
The National Energy Research Scientific Computing Center, which is
supported by the Office of Science of the U.S. Department of Energy
under Contract No. DE-AC02-05CH11231, provided staff, computational
resources, and data storage for this project.
NR 49
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U1 0
U2 12
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 DEC 1
PY 2011
VL 742
IS 2
AR L18
DI 10.1088/2041-8205/742/2/L18
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846SY
UT WOS:000296924700002
ER
PT J
AU Chew, BN
Campbell, JR
Reid, JS
Giles, DM
Welton, EJ
Salinas, SV
Liew, SC
AF Chew, Boon Ning
Campbell, James R.
Reid, Jeffrey S.
Giles, David M.
Welton, Ellsworth J.
Salinas, Santo V.
Liew, Soo Chin
TI Tropical cirrus cloud contamination in sun photometer data
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE AERONET; Aerosol particles; Cirrus clouds; Lidar; MPLNET; Southeast
Asia; Sun photometer
ID AEROSOL OPTICAL DEPTH; MICROPULSE LIDAR; MICROPHYSICAL PROPERTIES; PART
I; CLIMATOLOGY; FACILITY; AERONET; LAYER; RETRIEVALS; EXTINCTION
AB Cirrus clouds are endemic to Southeast Asia and are a source of potential bias in regional passive aerosol remote sensing datasets. Here, performance of the cloud-screening algorithm for the ground-based Aerosol Robotic Network (AERONET) sun photometer data is evaluated for cirrus cloud contamination at Singapore (1.30 degrees N, 103.77 degrees E). Using twelve months of concurrent AERONET Level 1.5 and 2.0 cloud-screened aerosol optical depth (AOD) data, and collocated Level 1.0 Micro-Pulse Lidar Network (MPLNE'T) measurements, we investigate the baseline AOD bias due to cirrus cloud presence. Observations are considered for a primary sample of all data and a secondary sample where AERONET data are restricted to a zenith viewing angle <= 45 degrees. Cirrus clouds are present in zenith-viewing MPL profiles for 34% and 23% of these samples respectively. Based on approximations of cirrus cloud optical properties necessary to estimate cloud optical depth from the single-channel lidar signal, and assuming partial forward scattering of diffuse light by cirrus clouds into the sun photometer's field of view, we estimate a range in AOD bias due to unscreened cloud presence of 0.034 to 0.060 and 0.031 to 0.055 +/- 0.01 for the primary and secondary sample respectively. From the analysis of AERONET AOD for the angle-limited subset alone, we also derive a positive AOD bias of 0.034, which is comparable to the lower bounds for the estimated cloud bias reported for our datasets. These findings, which we attribute to the prevalence of cirrus clouds present from regional convection, are higher than previous reports of global AOD bias in the Moderate Resolution Infrared Spectroradiometer (MODIS) satellite-borne measurements due to residual cirrus cloud presence. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Chew, Boon Ning; Salinas, Santo V.; Liew, Soo Chin] Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Singapore 119260, Singapore.
[Campbell, James R.; Reid, Jeffrey S.] USN, Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA.
[Giles, David M.] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
[Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Micropulse Lidar Network, Greenbelt, MD 20771 USA.
RP Chew, BN (reprint author), Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Block S17,Level 2,10 Lower Kent Ridge Rd, Singapore 119260, Singapore.
EM crscbn@nus.edu.sg
RI Welton, Ellsworth/A-8362-2012; Campbell, James/C-4884-2012; Liew, Soo
Chin/C-9187-2011; Reid, Jeffrey/B-7633-2014; Chew, Boon Ning/M-2405-2016
OI Campbell, James/0000-0003-0251-4550; Liew, Soo Chin/0000-0001-8342-4682;
Reid, Jeffrey/0000-0002-5147-7955; Chew, Boon Ning/0000-0002-2933-7788
FU Agency for Science, Technology and Research (A*STAR); NASA; Office of
Naval Research (ONR); ONR Global; MPLNET [NNX10AE14G, NNG11HG12I]
FX The Centre for Remote Imaging, Sensing and Processing (CRISP) thanks the
Agency for Science, Technology and Research (A*STAR) for financial
support. This research was initiated during a CRISP visit to the U.S.
Naval Research Laboratory (NRL) at Monterey, California that was
sponsored by the NASA Interdisciplinary Sciences Program. The AERONET
and MPLNET instruments are deployed at Singapore as part of the 7 SEAS
field campaign, which is sponsored by the Office of Naval Research
(ONR), ONR Global and NASA. AERONET and MPLNET are supported by the NASA
Radiation Sciences Program. Additional funding for this research was
provided by the ONR 32 and 35 programs, and by MPLNET through Grants
NNX10AE14G and NNG11HG12I issued by the NASA Shared Services Center. The
authors thank B.N. Holben and T.F. Eck of the AERONET project at NASA
Goddard Space Flight Center for fruitful discussions, as well as the
constructive comments of two anonymous referees who participated in the
review process.
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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 DEC
PY 2011
VL 45
IS 37
BP 6724
EP 6731
DI 10.1016/j.atmosenv.2011.08.017
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 846WV
UT WOS:000296934800013
ER
PT J
AU Pau, S
Wolkovich, EM
Cook, BI
Davies, TJ
Kraft, NJB
Bolmgren, K
Betancourt, JL
Cleland, EE
AF Pau, Stephanie
Wolkovich, Elizabeth M.
Cook, Benjamin I.
Davies, T. Jonathan
Kraft, Nathan J. B.
Bolmgren, Kjell
Betancourt, Julio L.
Cleland, Elsa E.
TI Predicting phenology by integrating ecology, evolution and climate
science
SO GLOBAL CHANGE BIOLOGY
LA English
DT Review
DE environmental filtering; growing-degree day models; niche conservatism;
photoperiod; temperature sensitivity; temporal niche
ID TREE SPECIES RANGE; PHYLOGENETIC SIGNAL; FLOWERING PHENOLOGY; COMMUNITY
ECOLOGY; NICHE CONSERVATISM; FUNCTIONAL TRAITS; SPRING PHENOLOGY;
TROPICAL FORESTS; PLANT PHENOLOGY; LIFE-HISTORY
AB Forecasting how species and ecosystems will respond to climate change has been a major aim of ecology in recent years. Much of this research has focused on phenology - the timing of life-history events. Phenology has well-demonstrated links to climate, from genetic to landscape scales; yet our ability to explain and predict variation in phenology across species, habitats and time remains poor. Here, we outline how merging approaches from ecology, climate science and evolutionary biology can advance research on phenological responses to climate variability. Using insight into seasonal and interannual climate variability combined with niche theory and community phylogenetics, we develop a predictive approach for species' reponses to changing climate. Our approach predicts that species occupying higher latitudes or the early growing season should be most sensitive to climate and have the most phylogenetically conserved phenologies. We further predict that temperate species will respond to climate change by shifting in time, while tropical species will respond by shifting space, or by evolving. Although we focus here on plant phenology, our approach is broadly applicable to ecological research of plant responses to climate variability.
C1 [Pau, Stephanie] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA.
[Wolkovich, Elizabeth M.; Cleland, Elsa E.] Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92130 USA.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Davies, T. Jonathan] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[Kraft, Nathan J. B.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada.
[Bolmgren, Kjell] Lund Univ, Dept Biol, SE-22362 Lund, Sweden.
[Betancourt, Julio L.] US Geol Survey, Natl Res Program, Tucson, AZ 85719 USA.
RP Pau, S (reprint author), Natl Ctr Ecol Anal & Synth, 735 State St, Santa Barbara, CA 93101 USA.
EM pau@nceas.ucsb.edu
RI Kraft, Nathan/A-2817-2012; Cook, Benjamin/H-2265-2012; Bolmgren,
Kjell/E-1459-2016
OI Kraft, Nathan/0000-0001-8867-7806; Bolmgren, Kjell/0000-0001-9552-9684
FU National Center for Ecological Analysis and Synthesis (NCEAS); NSF
[EF-0553768]; University of California, Santa Barbara; State of
California; USA National Phenology Network [IOS-0639794]; NSERC
FX This work was conducted as part of the Forecasting Phenology working
group supported by the National Center for Ecological Analysis and
Synthesis (NCEAS), a Center funded by NSF (Grant #EF-0553768), the
University of California, Santa Barbara, and the State of California,
and was supported by the USA National Phenology Network and its NSF RCN
grant (IOS-0639794) and conducted while EMW was an NSF Postdoctoral
Research Fellow in Biology (DBI-0905806), SP was an NCEAS postdoctoral
associate and while NJBK was supported by the NSERC CREATE training
program in biodiversity research. Please see Appendix S3 for author
contributions. We thank A. Rogstad and J. Weltzin for assistance in
reviewing cues across fields, H. Kharouba, S. Mazer, C. Parmesan, K.
Gerst, and J. Morisette for comments on an earlier draft, and thank all
members of the working group for discussion and perspectives across
fields.
NR 78
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U2 277
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD DEC
PY 2011
VL 17
IS 12
BP 3633
EP 3643
DI 10.1111/j.1365-2486.2011.02515.x
PG 11
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 843XN
UT WOS:000296710600010
ER
PT J
AU Ozanyan, KB
Katz, E
Nagle, HT
Lumelsky, V
AF Ozanyan, Krikor B.
Katz, Evgeny
Nagle, H. Troy
Lumelsky, Vladimir
TI Tenth Anniversary Issue
SO IEEE SENSORS JOURNAL
LA English
DT Editorial Material
C1 [Ozanyan, Krikor B.] Univ Manchester, Sch Elect & Elect Engn, Manchester M13 9PL, Lancs, England.
[Ozanyan, Krikor B.] Univ Manchester, Photon Sci Inst, Manchester M13 9PL, Lancs, England.
[Katz, Evgeny] Clarkson Univ, Milton Kerker Chair Colloid Sci Chem & Biomol Sci, Potsdam, NY 13699 USA.
[Nagle, H. Troy] N Carolina State Univ, Dept Biomed Engn, Univ N Carolina Chapel Hill, Raleigh, NC 27695 USA.
[Lumelsky, Vladimir] Univ Wisconsin, Dept Mech Engn, Madison, WI 53706 USA.
[Lumelsky, Vladimir] NASA, Goddard Space Ctr, Greenbelt, MD 20771 USA.
RP Ozanyan, KB (reprint author), Univ Manchester, Sch Elect & Elect Engn, Manchester M13 9PL, Lancs, England.
EM k.ozanyan@manchester.ac.uk; ekatz@clarkson.edu; nagle@ncsu.edu;
lumelsky@mail630.gsfc.nasa.gov
NR 2
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U1 0
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1530-437X
J9 IEEE SENS J
JI IEEE Sens. J.
PD DEC
PY 2011
VL 11
IS 12
BP 3053
EP 3054
DI 10.1109/JSEN.2011.2168469
PG 2
WC Engineering, Electrical & Electronic; Instruments & Instrumentation;
Physics, Applied
SC Engineering; Instruments & Instrumentation; Physics
GA 840RW
UT WOS:000296459700001
ER
PT J
AU Ade, PAR
Aghanim, N
Arnaud, M
Ashdown, M
Aumont, J
Baccigalupi, C
Balbi, A
Banday, AJ
Barreiro, RB
Bartlett, JG
Battaner, E
Benabed, K
Benoit, A
Bernard, JP
Bersanelli, M
Bhatia, R
Bonaldi, A
Bonavera, L
Bond, JR
Borrill, J
Bouchet, FR
Bucher, M
Burigana, C
Butler, RC
Cabella, P
Cantalupo, CM
Cappellini, B
Cardoso, JF
Carvalho, P
Catalano, A
Cayon, L
Challinor, A
Chamballu, A
Chary, RR
Chen, X
Chiang, LY
Chiang, C
Christensen, PR
Clements, DL
Colombi, S
Couchot, F
Coulais, A
Crill, BP
Cuttaia, F
Danese, L
Davis, RJ
de Bernardis, P
de Rosa, A
de Zotti, G
Delabrouille, J
Delouis, JM
Desert, FX
Dickinson, C
Diego, JM
Dolag, K
Dole, H
Donzelli, S
Dore, O
Dorl, U
Douspis, M
Dupac, X
Efstathiou, G
Ensslin, TA
Eriksen, HK
Finelli, F
Forni, O
Fosalba, P
Frailis, M
Franceschi, E
Galeotta, S
Ganga, K
Giard, M
Giraud-Heraud, Y
Gonzalez-Nuevo, J
Gorski, KM
Gratton, S
Gregorio, A
Gruppuso, A
Haissinski, J
Hansen, FK
Harrison, D
Helou, G
Henrot-Versille, S
Hernandez-Monteagudo, C
Herranz, D
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hornstrup, A
Hovest, W
Hoyland, RJ
Huffenberger, KM
Huynh, M
Jaffe, AH
Jones, WC
Juvela, M
Keihanen, E
Keskitalo, R
Kisner, TS
Kneissl, R
Knox, L
Kurki-Suonio, H
Lagache, G
Lahteenmaki, A
Lamarre, JM
Lasenby, A
Laureijs, RJ
Lawrence, CR
Leach, S
Leahy, JP
Leonardi, R
Leon-Tavares, J
Leroy, C
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Macias-Perez, JF
MacTavish, CJ
Maffei, B
Maggio, G
Maino, D
Mandolesi, N
Mann, R
Maris, M
Marleau, F
Marshall, DJ
Martinez-Gonzalez, E
Masi, S
Massardi, M
Matarrese, S
Matthai, F
Mazzotta, P
McGehee, P
Meinhold, PR
Melchiorri, A
Melin, JB
Mendes, L
Mennella, A
Mitra, S
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, A
Naselsky, P
Natoli, P
Netterfield, CB
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
O'Dwyer, IJ
Osborne, S
Pajot, F
Paladini, R
Partridge, B
Pasian, F
Patanchon, G
Pearson, TJ
Perdereau, O
Perotto, L
Perrotta, F
Piacentini, F
Piat, M
Piffaretti, R
Plaszczynski, S
Platania, P
Pointecouteau, E
Polenta, G
Ponthieu, N
Poutanen, T
Pratt, GW
Prezeau, G
Prunet, S
Puget, JL
Rachen, JP
Reach, WT
Rebolo, R
Reinecke, M
Renault, C
Ricciardi, S
Riller, T
Ristorcelli, I
Rocha, G
Rosset, C
Rowan-Robinson, M
Rubino-Martin, JA
Rusholme, B
Sajina, A
Sandri, M
Santos, D
Savini, G
Schaefer, BM
Scott, D
Seiffert, MD
Shellard, P
Smoot, GF
Starck, JL
Stivoli, F
Stolyarov, V
Sudiwala, R
Sunyaev, R
Sygnet, JF
Tauber, JA
Tavagnacco, D
Terenzi, L
Toffolatti, L
Tomasi, M
Torre, JP
Tristram, M
Tuovinen, J
Turler, M
Umana, G
Valenziano, L
Valiviita, J
Varis, J
Vielva, P
Villa, F
Vittorio, N
Wade, LA
Wandelt, BD
White, SDM
Wilkinson, A
Yvon, D
Zacchei, A
Zonca, A
AF Ade, P. A. R.
Aghanim, N.
Arnaud, M.
Ashdown, M.
Aumont, J.
Baccigalupi, C.
Balbi, A.
Banday, A. J.
Barreiro, R. B.
Bartlett, J. G.
Battaner, E.
Benabed, K.
Benoit, A.
Bernard, J. -P.
Bersanelli, M.
Bhatia, R.
Bonaldi, A.
Bonavera, L.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Bucher, M.
Burigana, C.
Butler, R. C.
Cabella, P.
Cantalupo, C. M.
Cappellini, B.
Cardoso, J. -F.
Carvalho, P.
Catalano, A.
Cayon, L.
Challinor, A.
Chamballu, A.
Chary, R. -R.
Chen, X.
Chiang, L. -Y.
Chiang, C.
Christensen, P. R.
Clements, D. L.
Colombi, S.
Couchot, F.
Coulais, A.
Crill, B. P.
Cuttaia, F.
Danese, L.
Davis, R. J.
de Bernardis, P.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Delouis, J. -M.
Desert, F. -X.
Dickinson, C.
Diego, J. M.
Dolag, K.
Dole, H.
Donzelli, S.
Dore, O.
Doerl, U.
Douspis, M.
Dupac, X.
Efstathiou, G.
Ensslin, T. A.
Eriksen, H. K.
Finelli, F.
Forni, O.
Fosalba, P.
Frailis, M.
Franceschi, E.
Galeotta, S.
Ganga, K.
Giard, M.
Giraud-Heraud, Y.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gratton, S.
Gregorio, A.
Gruppuso, A.
Haissinski, J.
Hansen, F. K.
Harrison, D.
Helou, G.
Henrot-Versille, S.
Hernandez-Monteagudo, C.
Herranz, D.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Holmes, W. A.
Hornstrup, A.
Hovest, W.
Hoyland, R. J.
Huffenberger, K. M.
Huynh, M.
Jaffe, A. H.
Jones, W. C.
Juvela, M.
Keihanen, E.
Keskitalo, R.
Kisner, T. S.
Kneissl, R.
Knox, L.
Kurki-Suonio, H.
Lagache, G.
Lahteenmaki, A.
Lamarre, J. -M.
Lasenby, A.
Laureijs, R. J.
Lawrence, C. R.
Leach, S.
Leahy, J. P.
Leonardi, R.
Leon-Tavares, J.
Leroy, C.
Lilje, P. B.
Linden-Vornle, M.
Lopez-Caniego, M.
Lubin, P. M.
Macias-Perez, J. F.
MacTavish, C. J.
Maffei, B.
Maggio, G.
Maino, D.
Mandolesi, N.
Mann, R.
Maris, M.
Marleau, F.
Marshall, D. J.
Martinez-Gonzalez, E.
Masi, S.
Massardi, M.
Matarrese, S.
Matthai, F.
Mazzotta, P.
McGehee, P.
Meinhold, P. R.
Melchiorri, A.
Melin, J. -B.
Mendes, L.
Mennella, A.
Mitra, S.
Miville-Deschenes, M. -A.
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Murphy, A.
Naselsky, P.
Natoli, P.
Netterfield, C. B.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
O'Dwyer, I. J.
Osborne, S.
Pajot, F.
Paladini, R.
Partridge, B.
Pasian, F.
Patanchon, G.
Pearson, T. J.
Perdereau, O.
Perotto, L.
Perrotta, F.
Piacentini, F.
Piat, M.
Piffaretti, R.
Plaszczynski, S.
Platania, P.
Pointecouteau, E.
Polenta, G.
Ponthieu, N.
Poutanen, T.
Pratt, G. W.
Prezeau, G.
Prunet, S.
Puget, J. -L.
Rachen, J. P.
Reach, W. T.
Rebolo, R.
Reinecke, M.
Renault, C.
Ricciardi, S.
Riller, T.
Ristorcelli, I.
Rocha, G.
Rosset, C.
Rowan-Robinson, M.
Rubino-Martin, J. A.
Rusholme, B.
Sajina, A.
Sandri, M.
Santos, D.
Savini, G.
Schaefer, B. M.
Scott, D.
Seiffert, M. D.
Shellard, P.
Smoot, G. F.
Starck, J. -L.
Stivoli, F.
Stolyarov, V.
Sudiwala, R.
Sunyaev, R.
Sygnet, J. -F.
Tauber, J. A.
Tavagnacco, D.
Terenzi, L.
Toffolatti, L.
Tomasi, M.
Torre, J. -P.
Tristram, M.
Tuovinen, J.
Tuerler, M.
Umana, G.
Valenziano, L.
Valiviita, J.
Varis, J.
Vielva, P.
Villa, F.
Vittorio, N.
Wade, L. A.
Wandelt, B. D.
White, S. D. M.
Wilkinson, A.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck early results. VII. The Early Release Compact Source Catalogue
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmology: observations; surveys; catalogs; radio continuum: general;
submillimeter: general
ID PRE-LAUNCH STATUS; DISCRETE OBJECT DETECTION; PROBE WMAP OBSERVATIONS;
ASTRONOMICAL DATA SETS; SOURCE EXTRACTION; BAYESIAN-APPROACH;
RADIO-SOURCES; GALAXIES; PERFORMANCE; CLUSTERS
AB A brief description of the methodology of construction, contents and usage of the Planck Early Release Compact Source Catalogue ( ERCSC), including the Early Cold Cores (ECC) and the Early Sunyaev-Zeldovich (ESZ) cluster catalogue is provided. The catalogue is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is >= 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857GHz. The 10 sigma photometric flux density limit of the catalogue at vertical bar b vertical bar > 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of similar to 2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. In addition, two early release catalogs that contain 915 cold molecular cloud core candidates and 189 SZ cluster candidates that have been generated using multifrequency algorithms are presented. The entire source list, with more than 15 000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities.
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[Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland.
[Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
[Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.] Univ Paris 07, CNRS, UMR7164, Paris, France.
[Ashdown, M.; Carvalho, P.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile.
[Bonavera, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway.
[Challinor, A.; Shellard, P.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England.
[Melin, J. -B.; Piffaretti, R.; Starck, J. -L.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France.
[Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Marleau, F.; Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Sajina, A.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
[Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
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[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
[Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy.
[Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Balbi, A.; Cabella, P.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
[Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain.
[Kneissl, R.] ESO Vitacura, European So Observ, Santiago, Chile.
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[Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
[Partridge, B.] Haverford Coll Astron Dept, Haverford, PA USA.
[Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland.
[Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy.
[Bonaldi, A.; de Zotti, G.; Massardi, M.] Osserv Astron Padova, INAF, Padua, Italy.
[Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Maggio, G.; Maris, M.; Mennella, A.; Pasian, F.; Tavagnacco, D.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy.
[Bersanelli, M.; Cappellini, B.; Donzelli, S.; Maino, D.; Tomasi, M.] INAF IASF Milano, Milan, Italy.
[Stivoli, F.] Univ Paris 11, Rech Informat Lab, INRIA, F-91405 Orsay, France.
[Desert, F. -X.] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France.
[Tuerler, M.] Univ Geneva, ISDC Data Ctr Astrophys, Versoix, Switzerland.
[Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France.
[Aghanim, N.; Aumont, J.; Dole, H.; Douspis, M.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France.
[Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France.
[Fosalba, P.] Fac Ciencies, CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain.
[Chiang, L. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Donzelli, S.; Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Barreiro, R. B.; Diego, J. M.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Platania, P.] EURATOM, ENEA, CNR, Ist Fis Plasma, Milan, Italy.
[Bartlett, J. G.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Mitra, S.; O'Dwyer, I. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Davis, R. J.; Dickinson, C.; Leahy, J. P.; Maffei, B.; Wilkinson, A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Catalano, A.; Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
[Arnaud, M.; Piffaretti, R.; Pratt, G. W.; Starck, J. -L.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France.
[Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France.
[Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France.
[Couchot, F.; Haissinski, J.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, Lab Accelerateur Lineaire, CNRS IN2P3, F-91405 Orsay, France.
[Borrill, J.; Cantalupo, C. M.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Banday, A. J.; Dolag, K.; Doerl, U.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland.
[Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland.
[Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Savini, G.] UCL, Opt Sci Lab, London, England.
[Baccigalupi, C.; Bonavera, L.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Mann, R.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA.
[Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Schaefer, B. M.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Reach, W. T.] Stratospher Observ Infrared Astron, Univ Space Res Assoc, Moffett Field, CA 94035 USA.
[Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain.
[Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA.
[Gorski, K. M.] Univ Warsaw Observ, Warsaw, Poland.
RP Chary, RR (reprint author), CALTECH, Ctr Infrared Proc & Anal, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM rchary@caltech.edu
RI Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015;
Valiviita, Jussi/A-9058-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi,
Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov,
Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov,
Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta,
Pasquale/B-1225-2016; bonavera, laura/E-9368-2017; Martinez-Gonzalez,
Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Lilje,
Per/A-2699-2012; Gregorio, Anna/J-1632-2012; Lopez-Caniego,
Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki,
Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti,
Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner,
Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon,
Dominique/D-2280-2015; Butler, Reginald/N-4647-2015;
OI Pasian, Fabio/0000-0002-4869-3227; WANDELT,
Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana,
Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis,
Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283;
Gregorio, Anna/0000-0003-4028-8785; Polenta,
Gianluca/0000-0003-4067-9196; Rubino-Martin, Jose
Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; de
Bernardis, Paolo/0000-0001-6547-6446; Forni,
Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412;
Maris, Michele/0000-0001-9442-2754; Franceschi,
Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104;
Pearson, Timothy/0000-0001-5213-6231; Gruppuso,
Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693;
Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi,
Maurizio/0000-0002-1448-6131; Piacentini, Francesco/0000-0002-5444-9327;
Stolyarov, Vladislav/0000-0001-8151-828X; Mazzotta,
Pasquale/0000-0002-5411-1748; bonavera, laura/0000-0001-8039-3876;
Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; Vielva, Patricio/0000-0003-0051-272X;
Toffolatti, Luigi/0000-0003-2645-7386; Herranz,
Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272;
Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416;
TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794;
Reach, William/0000-0001-8362-4094; Zacchei, Andrea/0000-0003-0396-1192;
Hivon, Eric/0000-0003-1880-2733; Butler, Reginald/0000-0003-4366-5996;
Sandri, Maura/0000-0003-4806-5375; Cuttaia,
Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099;
Burigana, Carlo/0000-0002-3005-5796; Bouchet,
Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043;
Villa, Fabrizio/0000-0003-1798-861X; Galeotta,
Samuele/0000-0002-3748-5115
FU NASA; ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy);
DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA (Spain); Tekes; AoF; CSC
(Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark);
SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES
(Portugal); DEISA (EU)
FX The production of the Planck Early Release Compact Source Catalogue was
funded by NASA and carried out at the US Planck Data Center at the
Infrared Processing and Analysis Center (IPAC), California Institute of
Technology, on behalf of and in collaboration with the LFI and HFI Data
Processing Centers and with many contributions by members of the Planck
Collaboration. The Planck Collaboration acknowledges the support of:
ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy);
NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain);
Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU
Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland);
FCT/MCTES (Portugal); and DEISA (EU). A description of the Planck
Collaboration and a list of its members with the technical or scientific
activities they have been involved into, can be found at
http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborati
on
NR 64
TC 177
Z9 177
U1 0
U2 18
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 DEC
PY 2011
VL 536
AR A7
DI 10.1051/0004-6361/201116474
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100008
ER
PT J
AU Yates, EL
Schiro, K
Lowenstein, M
Sheffner, EJ
Iraci, LT
Tadic, JM
Kuze, A
AF Yates, Emma L.
Schiro, Kathleen
Lowenstein, Max
Sheffner, Edwin J.
Iraci, Laura T.
Tadic, Jovan M.
Kuze, Akihiko
TI Carbon Dioxide and Methane at a Desert Site-A Case Study at Railroad
Valley Playa, Nevada, USA
SO ATMOSPHERE
LA English
DT Article
DE CO2; CH4; playa
AB Ground based in-situ measurements of carbon dioxide (CO2) and methane (CH4) at the dry lakebed at Railroad Valley (RRV) playa, Nevada, USA (38 degrees 30.234' N, 115 degrees 41.604' W, elevation 1437 m) were conducted over a five day period from 20-25 June 2010. The playa is a flat, desert site with virtually no vegetation, an overall size of 15 km x 15 km and is approximately 110 km south-west of the nearest city, Ely (elevation 1962 m, inhabitants 4000). The measurements were taken in support of the vicarious calibration experiment to validate column-averaged dry air mole fractions of CO2 and CH4 (X-CO2 and X-CH4) retrieved from the Greenhouse Gases Observing Satellite (GOSAT) which was launched in January 2009. This work reports on ground-based in-situ measurements of CO2 and CH4 from RRV playa and describes comparisons made between in-situ data and X-CO2 and X-CH4 from GOSAT.
C1 [Yates, Emma L.; Schiro, Kathleen; Lowenstein, Max; Sheffner, Edwin J.; Iraci, Laura T.; Tadic, Jovan M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schiro, Kathleen] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Kuze, Akihiko] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan.
RP Yates, EL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM emma.l.yates@nasa.gov; kschiro@ucla.edu; max.loewenstein@nasa.gov;
edwin.j.sheffner@nasa.gov; laura.t.iraci@nasa.gov; jovan.tadic@nasa.gov;
kuze.akihiko@jaxa.jp
RI KUZE, AKIHIKO/J-2074-2016; Tadic, Jovan/P-3677-2016
OI KUZE, AKIHIKO/0000-0001-5415-3377;
FU NASA's Earth Science Division; Oak Ridge Associated Universities (ORAU)
through the NASA Postdoctoral Program
FX We specifically acknowledge the cooperation and efforts of the personnel
involved in the Railroad Valley vicarious calibration experiment from
Atmospheric CO2 Observations from Space (ACOS), Japan
Aerospace Exploration Agency (JAXA), National Institute for
Environmental Studies (NIES) and Colorado State University (CSU),
particulary the work of Hiroshi Suto of JAXA, NIES GOSAT project office,
David Crisp and Carol Bruegge of ACOS. We also thank the University of
Arizona Remote Sensing Group for making the research facilities at
Railroad Valley available. We acknowledge financial support from NASA's
Earth Science Division and Oak Ridge Associated Universities (ORAU)
through the NASA Postdoctoral Program (E.L.Y., J.M.T.). Helpful comments
from two anonymous reviewers are appreciated.
NR 29
TC 3
Z9 3
U1 3
U2 11
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2073-4433
J9 ATMOSPHERE-BASEL
JI Atmosphere
PD DEC
PY 2011
VL 2
IS 4
BP 702
EP 714
DI 10.3390/atmos2040702
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA V29ET
UT WOS:000208732400007
ER
PT J
AU van den Hurk, B
Best, M
Dirmeyer, P
Pitman, A
Polcher, J
Santanello, J
AF van den Hurk, Bart
Best, Martin
Dirmeyer, Paul
Pitman, Andy
Polcher, Jan
Santanello, Joe
TI ACCELERATION OF LAND SURFACE MODEL DEVELOPMENT OVER A DECADE OF GLASS
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID PARAMETERIZATION SCHEMES PILPS; LATITUDE HYDROLOGICAL PROCESSES;
GENERAL-CIRCULATION MODELS; RIVER-BASIN EXPERIMENT; SOIL WETNESS
PROJECT; DIURNAL TIME SCALES; TORNE-KALIX BASIN; BIOSPHERE MODEL; PHASE;
MOISTURE
C1 [van den Hurk, Bart] KNMI, NL-3730 AE De Bilt, Netherlands.
[Dirmeyer, Paul] Ctr Ocean Land Atmosphere Studies, Calverton, MD USA.
[Pitman, Andy] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW, Australia.
[Polcher, Jan] CNRS, Meteorol Dynam Lab, Paris, France.
[Santanello, Joe] NASA, Hydrospher & Biospher Sci Lab, Greenbelt, MD USA.
RP van den Hurk, B (reprint author), KNMI, POB 201, NL-3730 AE De Bilt, Netherlands.
EM hurkvd@knmi.nl
RI Santanello, Joseph/D-4438-2012; Pitman, Andrew/A-7353-2011; Dirmeyer,
Paul/B-6553-2016;
OI Santanello, Joseph/0000-0002-0807-6590; Pitman,
Andrew/0000-0003-0604-3274; Dirmeyer, Paul/0000-0003-3158-1752; Best,
Martin/0000-0003-4468-876X
NR 39
TC 29
Z9 29
U1 2
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD DEC
PY 2011
VL 92
IS 12
BP 1593
EP 1600
DI 10.1175/BAMS-D-11-00007.1
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 876TM
UT WOS:000299130600012
ER
PT J
AU Milner-White, EJ
Russell, MJ
AF Milner-White, E. James
Russell, Michael J.
TI Functional Capabilities of the Earliest Peptides and the Emergence of
Life
SO GENES
LA English
DT Article
DE catgrips; emergence of life; hydrothermal mound; nests; niches; peptides
ID ANION-BINDING MOTIFS; ALPHA-SHEET; AMINO-ACID; SUCCESSIVE RESIDUES;
HYDROTHERMAL VENT; ABIOTIC SYNTHESIS; STRUCTURAL BASIS; EARLY EVOLUTION;
PROTEINS; ORIGIN
AB Considering how biological macromolecules first evolved, probably within a marine environment, it seems likely the very earliest peptides were not encoded by nucleic acids, or at least not via the genetic code as we know it. An objective of the present work is to demonstrate that sequence-independent peptides, or peptides with variable and unreliable lengths and sequences, have the potential to perform a variety of chemically useful functions such as anion and cation binding and membrane and channel formation as well as simple types of catalysis. These functions tend to be performed with the assistance of the main chain CONH atoms rather than the more variable or limited side chain atoms of the peptides presumed to exist then.
C1 [Milner-White, E. James] Univ Glasgow, Coll Med Vet & Life Sci, Glasgow G12 8QQ, Lanark, Scotland.
[Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Milner-White, EJ (reprint author), Univ Glasgow, Coll Med Vet & Life Sci, Glasgow G12 8QQ, Lanark, Scotland.
EM J.Milner-White@bio.gla.ac.uk; mrussell@jpl.nasa.gov
FU NASA Exobiology and Evolutionary Biology award [NNH06ZDA001N]; NASA
Astrobiology, Science and Technology Exploration Program (ASTEP); NASA
Astrobiology Institute (NAI-Icy Worlds); US government
FX We thank Laurie Barge, Isik Kanik, Shawn McGlynn, Randy Mielke, Wolfgang
Nitschke and Lauren White for discussions. MJR's research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration: with joint support by NASA Exobiology and Evolutionary
Biology award (NNH06ZDA001N) and NASA Astrobiology, Science and
Technology Exploration Program (ASTEP) as well as that from the NASA
Astrobiology Institute (NAI-Icy Worlds). US government sponsorship is
acknowledged. The copyright in work done by JPL authors is held by the
California Institute of Technology.
NR 83
TC 14
Z9 14
U1 1
U2 10
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2073-4425
J9 GENES-BASEL
JI Genes
PD DEC
PY 2011
VL 2
IS 4
BP 671
EP 688
DI 10.3390/genes2040671
PG 18
WC Genetics & Heredity
SC Genetics & Heredity
GA V36XZ
UT WOS:000209242200002
PM 24710286
ER
PT J
AU Wright, R
Glaze, L
Baloga, SM
AF Wright, Robert
Glaze, Lori
Baloga, Stephen M.
TI Constraints on determining the eruption style and composition of
terrestrial lavas from space
SO GEOLOGY
LA English
DT Article
ID FLOWS; VOLCANO; MODEL; IO
AB The surface temperatures of active lavas relate to cooling rates, chemistry, and eruption style. We analyzed 61 hyperspectral satellite images acquired by the National Aeronautics and Space Administration's Earth Observing-1 (EO-1) Hyperion imaging spectrometer to document the surface temperature distributions of active lavas erupted at 13 volcanoes. Images were selected to encompass the range of common lava eruption styles, specifically, lava fountains, flows, lakes, and domes. Our results reveal temperature distributions for terrestrial lavas that correlate with composition (i.e., a statistically significant difference in the highest temperatures retrieved for mafic lavas and intermediate and felsic lavas) and eruption style. Maximum temperatures observed for mafic lavas are similar to 200 degrees C higher than for intermediate and felsic lavas. All eruption styles exhibit a low-temperature mode at similar to 300 degrees C; lava fountains and 'a' a flows also exhibit a higher-temperature mode at similar to 700 degrees C. The observed differences between the temperatures are consistent with the contrasting rates at which the lava surfaces are thermally renewed. Eruption styles that allow persistent and pervasive thermal renewal of the lava surface (e.g., fractured crusts on channel-fed 'a' (a) over bar flows) exhibit a bimodal temperature distribution; eruption styles that do not (e.g., the continuous skin of p (a) over bar hoehoe lavas) exhibit a single mode. We conclude that insights into composition and eruption style can only be gained remotely by analyzing a large spatio-temporal sample of data. This has implications for determining composition and eruption style at the Jovian moon Io, for which no in situ validation is available.
C1 [Wright, Robert] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Glaze, Lori] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baloga, Stephen M.] Proxemy Res Inc, Gaithersburg, MD 20882 USA.
RP Wright, R (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
EM wright@higp.hawaii.edu
RI Glaze, Lori/D-1314-2012
FU National Aeronautics and Space Administration (NASA) [NNX08AG03G,
NNX10AT65G, NNZ10AP63G, WBS 811073.02.01.04.44]
FX Wright was supported by the National Aeronautics and Space
Administration (NASA) (NNX08AG03G and NNX10AT65G). Glaze was supported
by the NASA Planetary Geology and Geophysics Program (WBS
811073.02.01.04.44). Baloga was supported by NASA Grant NNZ10AP63G.
Hyperion data were acquired as part of the Jet Propulsion Laboratory's
Sensor Webs project. We thank three reviewers for improving the
presentation of this work. This paper is Hawai'i Institute of Geophysics
and Planetology Publication 1894 and School of Ocean, Earth Science, and
Technology Publication 8208.
NR 22
TC 7
Z9 9
U1 0
U2 1
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD DEC
PY 2011
VL 39
IS 12
BP 1127
EP 1130
DI 10.1130/G32341.1
PG 4
WC Geology
SC Geology
GA 844ZZ
UT WOS:000296793900010
ER
PT J
AU Moran, PJ
Ellsworth, D
AF Moran, Patrick J.
Ellsworth, David
TI Visualization of AMR Data With Multi-Level Dual-Mesh Interpolation
SO IEEE TRANSACTIONS ON VISUALIZATION AND COMPUTER GRAPHICS
LA English
DT Article; Proceedings Paper
CT IEEE Visualization Conference (Vis)/IEEE Information Visualization
Conference (InfoVis)
CY OCT 23-28, 2011
CL Providence, RI
SP IEEE
DE Adaptive mesh refinement; AMR; Enzo; interpolation; ray casting;
isosurfaces; dual meshes; stitching cells
ID REFINEMENT; HYDRODYNAMICS
AB We present a new technique for providing interpolation within cell-centered Adaptive Mesh Refinement (AMR) data that achieves C-0 continuity throughout the 3D domain. Our technique improves on earlier work in that it does not require that adjacent patches differ by at most one refinement level. Our approach takes the dual of each mesh patch and generates "stitching cells" on the fly to fill the gaps between dual meshes. We demonstrate applications of our technique with data from Enzo, an AMR cosmological structure formation simulation code. We show ray-cast visualizations that include contributions from particle data (dark matter and stars, also output by Enzo) and gridded hydrodynamic data. We also show results from isosurface studies, including surfaces in regions where adjacent patches differ by more than one refinement level.
C1 [Moran, Patrick J.; Ellsworth, David] NASA, Comp Sci Corp, Ames Res Ctr, Washington, DC 20546 USA.
RP Moran, PJ (reprint author), NASA, Comp Sci Corp, Ames Res Ctr, Washington, DC 20546 USA.
EM patrick.moran@nasa.gov; david.ellsworth@nasa.gov
NR 22
TC 4
Z9 4
U1 1
U2 4
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1077-2626
J9 IEEE T VIS COMPUT GR
JI IEEE Trans. Vis. Comput. Graph.
PD DEC
PY 2011
VL 17
IS 12
BP 1862
EP 1871
PG 10
WC Computer Science, Software Engineering
SC Computer Science
GA 837XD
UT WOS:000296241900015
PM 22034303
ER
PT J
AU Ding, BL
Zhao, B
Lin, CX
Han, JW
Zhai, CX
Srivastava, A
Oza, NC
AF Ding, Bolin
Zhao, Bo
Lin, Cindy Xide
Han, Jiawei
Zhai, Chengxiang
Srivastava, Ashok
Oza, Nikunj C.
TI Efficient Keyword-Based Search for Top-K Cells in Text Cube
SO IEEE TRANSACTIONS ON KNOWLEDGE AND DATA ENGINEERING
LA English
DT Article
DE Keyword search; multidimensional text data; data cube
ID RELATIONAL DATABASES
AB Previous studies on supporting free-form keyword queries over RDBMSs provide users with linked structures (e.g., a set of joined tuples) that are relevant to a given keyword query. Most of them focus on ranking individual tuples from one table or joins of multiple tables containing a set of keywords. In this paper, we study the problem of keyword search in a data cube with text-rich dimension(s) (so-called text cube). The text cube is built on a multidimensional text database, where each row is associated with some text data (a document) and other structural dimensions (attributes). A cell in the text cube aggregates a set of documents with matching attribute values in a subset of dimensions. We define a keyword-based query language and an IR-style relevance model for scoring/ranking cells in the text cube. Given a keyword query, our goal is to find the top-k most relevant cells. We propose four approaches: inverted-index one-scan, document sorted-scan, bottom-up dynamic programming, and search-space ordering. The search-space ordering algorithm explores only a small portion of the text cube for finding the top-k answers, and enables early termination. Extensive experimental studies are conducted to verify the effectiveness and efficiency of the proposed approaches.
C1 [Ding, Bolin; Zhao, Bo; Lin, Cindy Xide; Han, Jiawei; Zhai, Chengxiang] Univ Illinois, Dept Comp Sci, Urbana, IL 61801 USA.
[Srivastava, Ashok; Oza, Nikunj C.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Ding, BL (reprint author), Univ Illinois, Dept Comp Sci, 201 N Goodwin Ave, Urbana, IL 61801 USA.
EM bding3@uiuc.edu; bozhao3@uiuc.edu; xidelin2@uiuc.edu; hanj@uiuc.edu;
czhai@uiuc.edu; ashok@email.arc.nasa.gov; nikunj.c.oza@nasa.gov
FU NASA [NNX08AC35A]; US National Science Foundation (NSF) [IS-09-05215];
HP; Microsoft; Network Science Collaborative Technology Alliance Program
(NS-CTA/INARC) of US Army Research Lab (ARL) [W911NF-09-2-0053]
FX The work was supported in part by the NASA Aviation Safety Program,
Integrated Vehicle Health Management Project by NASA grant NNX08AC35A,
the US National Science Foundation (NSF) grant IS-09-05215, an HP
Research grant, Microsoft research Women's Scholarship, and the Network
Science Collaborative Technology Alliance Program (NS-CTA/INARC) of US
Army Research Lab (ARL) under the contract number W911NF-09-2-0053. Any
opinions, findings, and conclusions expressed here are those of the
authors and do not necessarily reflect the views of the funding
agencies. The US Government is authorized to reproduce and distribute
reprints for Government purposes notwithstanding any copyright notation
here on. This paper is an extended version of [39]. The authors thank
the anonymous reviewers for their numerous insights and suggestions that
immensely improved the paper.
NR 39
TC 2
Z9 2
U1 0
U2 5
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1041-4347
EI 1558-2191
J9 IEEE T KNOWL DATA EN
JI IEEE Trans. Knowl. Data Eng.
PD DEC
PY 2011
VL 23
IS 12
BP 1795
EP 1810
DI 10.1109/TKDE.2011.34
PG 16
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA 834RB
UT WOS:000295979600004
ER
PT J
AU Valentini, P
Schwartzentruber, TE
Cozmuta, I
AF Valentini, Paolo
Schwartzentruber, Thomas E.
Cozmuta, Ioana
TI ReaxFF Grand Canonical Monte Carlo simulation of adsorption and
dissociation of oxygen on platinum (111)
SO SURFACE SCIENCE
LA English
DT Article
DE Grand Canonical Monte Carlo; Reactive force field; Heterogeneous
catalysis
ID REACTIVE FORCE-FIELD; PT(111) SURFACE; ATOMIC OXYGEN; LATERAL
INTERACTIONS; MOLECULAR-DYNAMICS; OXIDATION; DESORPTION; ENERGETICS;
COVERAGES; KINETICS
AB Atomic-level Grand Canonical Monte Carlo (GCMC) simulations equipped with a reactive force field (ReaxFF) are used to study atomic oxygen adsorption on a Pt(111) surface. The off-lattice GCMC calculations presented here rely solely on the interatomic potential and do not necessitate the pre-computation of surface adlayer structures and their interpolation. As such, they provide a predictive description of adsorbate phases. In this study, validation is obtained with experimental evidence (steric heats of adsorption and isotherms) as well as DFT-based state diagrams available in the literature. The ReaxFF computed steric heats of adsorption agree well with experimental data, and this study clearly shows that indirect dissociative adsorption of O(2) on Pt( 111) is an activated process at non-zero coverages, with an activation energy that monotonically increases with coverage. At a coverage of 0.25 ML, a highly ordered p(2 x 2) adlayer is found, in agreement with several low-energy electron diffraction observations. Isotherms obtained from the GCMC simulations compare qualitatively and quantitatively well with previous OF-based state diagrams, but are in disagreement with the experimental data sets available. ReaxFF GCMC simulations at very high coverages show that O atoms prefer to bind in fcc hollow sites, at least up to 0.8 ML considered in the present work. At moderate coverages, little to no disorder appears in the Pt lattice. At high coverages, some Pt atoms markedly protrude out of the surface plane. This observation is in qualitative agreement with recent STM images of an oxygen covered Pt surface. The use of the GCMC technique based on a transferable potential is particularly valuable to produce more realistic systems (adsorbent and adsorbate) to be used in subsequent dynamical simulations (Molecular Dynamics) to address recombination reactions (via either Eley-Rideal or Langmuir-Hinshelwood mechanisms) on variously covered surfaces. By using GCMC and Molecular Dynamics simulations, the ReaxFF force field can be a valuable tool for understanding heterogeneous catalysis on a solid surface. Finally, the use of a reactive potential is a necessary requirement to investigate problems where dissociative adsorption occurs, as typical of many important catalytic processes. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Valentini, Paolo; Schwartzentruber, Thomas E.] Univ Minnesota, Coll Sci & Engn, Dept Aerosp Engn & Mech, Minneapolis, MN 55455 USA.
[Cozmuta, Ioana] NASA, Ames Res Ctr, ERC Inc, Moffett Field, CA 94035 USA.
RP Valentini, P (reprint author), Univ Minnesota, Coll Sci & Engn, Dept Aerosp Engn & Mech, Minneapolis, MN 55455 USA.
EM vale@aem.umn.edu; schwartz@aem.umn.edu; ioana.cozmuta@nasa.gov
RI Valentini, Paolo/A-6660-2011
FU Air Force Office of Scientific Research (AFOSR) [FA9550-09-1-0157];
University of Minnesota
FX We are grateful to Prof. Adri van Duin (Penn State) for his help with
the ReaxFF potential, and for providing us with the parameters for
simulating the system of interest. The research is supported by the Air
Force Office of Scientific Research (AFOSR) under Grant No.
FA9550-09-1-0157. The views and conclusions contained herein are those
of the authors and should not be interpreted as necessarily representing
the official policies or endorsements, either expressed or implied, of
the AFOSR or the U.S. Government. P. V. would like to acknowledge
partial support from the 2009-2010 Doctoral Dissertation Fellowship of
the University of Minnesota.
NR 46
TC 14
Z9 14
U1 1
U2 39
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0039-6028
J9 SURF SCI
JI Surf. Sci.
PD DEC
PY 2011
VL 605
IS 23-24
BP 1941
EP 1950
DI 10.1016/j.susc.2011.07.005
PG 10
WC Chemistry, Physical; Physics, Condensed Matter
SC Chemistry; Physics
GA 837EY
UT WOS:000296175100004
ER
PT J
AU Calle, CI
Buhler, CR
Johansen, MR
Hogue, MD
Snyder, SJ
AF Calle, C. I.
Buhler, C. R.
Johansen, M. R.
Hogue, M. D.
Snyder, S. J.
TI Active dust control and mitigation technology for lunar and Martian
exploration
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Lunar exploration; Mars exploration; Planetary exploration; Exploration
missions; Dust mitigation; Dust control; Dust removal
AB Mars is covered with a layer of dust that has been homogenized by global dust storms. Dust, levitated by these storms as well as by the frequent dust devils, is the dominant weather phenomenon on Mars. NASA's Mars exploration rovers have shown that atmospheric dust falling on solar panels can decrease their efficiency to the point of rendering the rover unusable. Dust covering the surface of the moon is expected to be electrostatically charged due to the solar wind, cosmic rays, and the solar radiation itself through the photoelectric effect. Electrostatically charged dust has a large tendency to adhere to surfaces. The Apollo missions to the moon showed that lunar dust adhesion can hinder manned and unmanned exploration activities. In this paper, we report on our efforts to develop an electrodynamic dust shield to prevent the accumulation of dust on surfaces and to remove dust already adhering to those surfaces. The technology uses electrostatic and dielectrophoretic forces to carry dust particles off surfaces and to generate an electrodynamic shield that prevents further accumulation of dust. The concept of the electrodynamic dust shield was introduced by NASA in the late 1960s and later reduced to practice during the 1970s for terrestrial applications. In 2003, our laboratory, in collaboration with several universities, applied this technology to space applications, specifically to remove dust from solar panels on Mars. We show how, with an appropriate design, we can prevent the electrostatic breakdown at the low Martian atmospheric pressures. We are also able to show that uncharged dust can be lifted and removed from surfaces under simulated Martian environmental conditions. We have also been able to develop a version of the electrodynamic dust shield working under hard vacuum conditions that simulate the lunar environment. We have implemented the electrodynamic dust shield on solar arrays, optical systems, spectrometers, viewports, thermal radiators, batteries, and power systems, as well as on fabrics for spacesuits. We present data on the design and optimization of the electrodynamic dust shields and provide data on the performance of the different implementations of the technology for lunar and Martian exploration activities. Published by Elsevier Ltd.
C1 [Calle, C. I.; Johansen, M. R.; Hogue, M. D.] NASA, Kennedy Space Ctr, FL 32899 USA.
[Buhler, C. R.; Snyder, S. J.] ASRC Aerosp, Kennedy Space Ctr, FL 32899 USA.
RP Calle, CI (reprint author), NASA, Kennedy Space Ctr, FL 32899 USA.
EM carlos.i.calle@nasa.gov
NR 14
TC 14
Z9 14
U1 3
U2 32
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 DEC
PY 2011
VL 69
IS 11-12
BP 1082
EP 1088
DI 10.1016/j.actaastro.2011.06.010
PG 7
WC Engineering, Aerospace
SC Engineering
GA 830LH
UT WOS:000295658000019
ER
PT J
AU Lee, C
Lawson, WG
Richardson, MI
Anderson, JL
Collins, N
Hoar, T
Mischna, M
AF Lee, C.
Lawson, W. G.
Richardson, M. I.
Anderson, J. L.
Collins, N.
Hoar, T.
Mischna, M.
TI Demonstration of ensemble data assimilation for Mars using DART,
MarsWRF, and radiance observations from MGS TES
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID QUASI-GEOSTROPHIC MODEL; KALMAN FILTER; MARTIAN ATMOSPHERE;
METEOROLOGICAL DATA; THERMAL STRUCTURE; DUST STORM; IMPLEMENTATION;
CLIMATE; SCHEME
AB We describe a global atmospheric data assimilation scheme that has been adapted for use with a Martian General Circulation Model (GCM), with the ultimate goal of creating globally and temporally interpolated "reanalysis" data sets from planetary atmospheric observations. The system uses the Data Assimilation Research Testbed (DART) software to apply an Ensemble Kalman Filter (EnKF) to the MarsWRF GCM. Specific application to Mars also required the development of a radiance forward model for near-nadir Thermal Emission Spectrometer (TES) observations. Preliminary results from an assimilation of 40 sols of TES radiance data, taken around L-s = 150 degrees (August 1999, Mars Year 24), are provided. 1.3 million TES observations are ingested and used to improve the state prediction by the GCM, with bias and error reductions obtained throughout the state vector. Results from the assimilation suggest steepening of the latitudinal and vertical thermal gradients with concurrent strengthening of the mid-latitude zonal jets, and a slower recession of the southern polar ice edge than predicted by the unaided GCM. Limitations of the prescribed dust model are highlighted by the presence of an atmospheric radiance bias. Preliminary results suggest the prescribed dust vertical profile might not be suitable for all seasons, in accordance with more recent observations of the vertical distribution of dust by the Mars Climate Sounder. The tools developed using this DA system are available at http://www.marsclimatecenter.com. A tutorial and example TES radiance assimilation are also provided.
C1 [Lee, C.; Richardson, M. I.] Ashima Res, Pasadena, CA 91101 USA.
[Lawson, W. G.] Point Carbon, Washington, DC 20002 USA.
[Anderson, J. L.; Collins, N.; Hoar, T.] Natl Ctr Atmospher Res, Inst Math Appl Geosci, Boulder, CO 80307 USA.
[Mischna, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lee, C (reprint author), Ashima Res, 600 S Lake Ave,Ste 104, Pasadena, CA 91101 USA.
EM lee@ashimaresearch.com
FU NASA [NNX09AN39G]; Mars Climate Sounder (MCS) project
FX This work was primarily funded by the NASA Applied Information Systems
Research (AISR) Program under grant NNX09AN39G. Additional support was
provided by the Mars Climate Sounder (MCS) project. We thank the three
reviewers for their comments that have led to significant improvements
in this manuscript.
NR 54
TC 12
Z9 12
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD NOV 29
PY 2011
VL 116
AR E11011
DI 10.1029/2011JE003815
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 856OM
UT WOS:000297652300001
ER
PT J
AU Righter, K
O'Brien, DP
AF Righter, K.
O'Brien, D. P.
TI Terrestrial planet formation
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
ID HIGH-RESOLUTION SIMULATIONS; EARLY SOLAR-SYSTEM; EARTH-LIKE PLANETS;
PROTOPLANETARY NEBULA; CLOSE ENCOUNTERS; CORE FORMATION; PLANETESIMALS;
ACCRETION; EVOLUTION; ISOTOPES
AB Advances in our understanding of terrestrial planet formation have come from a multidisciplinary approach. Studies of the ages and compositions of primitive meteorites with compositions similar to the Sun have helped to constrain the nature of the building blocks of planets. This information helps to guide numerical models for the three stages of planet formation from dust to planetesimals (similar to 10(6) y), followed by planetesimals to embryos (lunar to Mars-sized objects; few x 10(6) y), and finally embryos to planets (10(7)-10(8) y). Defining the role of turbulence in the early nebula is a key to understanding the growth of solids larger than meter size. The initiation of runaway growth of embryos from planetesimals ultimately leads to the growth of large terrestrial planets via large impacts. Dynamical models can produce inner Solar System configurations that closely resemble our Solar System, especially when the orbital effects of large planets (Jupiter and Saturn) and damping mechanisms, such as gas drag, are included. Experimental studies of terrestrial planet interiors provide additional constraints on the conditions of differentiation and, therefore, origin. A more complete understanding of terrestrial planet formation might be possible via a combination of chemical and physical modeling, as well as obtaining samples and new geophysical data from other planets (Venus, Mars, or Mercury) and asteroids.
C1 [Righter, K.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[O'Brien, D. P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Righter, K (reprint author), NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
FU NASA
FX We thank M. Thiemens for the invitation to contribute this paper. K. R.
is supported through a NASA Cosmochemistry Research and Technology
Operating Plan (RTOP) and D.P.O. is supported by NASA's Planetary
Geology and Geophysics research program. The reviews of R.J. Walker, E.
Asphaug, and an anonymous journal reviewer helped to improve the clarity
of the presentation. This paper is Planetary Science Institute (PSI)
Contribution 509.
NR 84
TC 9
Z9 10
U1 3
U2 25
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 NOV 29
PY 2011
VL 108
IS 48
BP 19165
EP 19170
DI 10.1073/pnas.1013480108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 853ZB
UT WOS:000297463100021
PM 21709256
ER
PT J
AU Cody, GD
Heying, E
Alexander, CMO
Nittler, LR
Kilcoyne, ALD
Sandford, SA
Stroud, RM
AF Cody, George D.
Heying, Emily
Alexander, Conel M. O.
Nittler, Larry R.
Kilcoyne, A. L. David
Sandford, Scott A.
Stroud, Rhonda M.
TI Establishing a molecular relationship between chondritic and cometary
organic solids
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
ID ISOTOPIC COMPOSITIONS; INTERPLANETARY DUST; MURCHISON METEORITE; SOLAR
NEBULA; ICE ANALOGS; C-13 NMR; MATTER; 81P/WILD-2; INTERSTELLAR;
SPECTROSCOPY
AB Multidimensional solid-state NMR spectroscopy is used to refine the identification and abundance determination of functional groups in insoluble organic matter (IOM) isolated from a carbonaceous chondrite (Murchison, CM2). It is shown that IOM is composed primarily of highly substituted single ring aromatics, substituted furan/pyran moieties, highly branched oxygenated aliphatics, and carbonyl groups. A pathway for producing an IOM-like molecular structure through formaldehyde polymerization is proposed and tested experimentally. Solid-state C-13 NMR analysis of aqueously altered formaldehyde polymer reveals considerable similarity with chondritic IOM. Carbon X-ray absorption near edge structure spectroscopy of formaldehyde polymer reveals the presence of similar functional groups across certain Comet 81P/Wild 2 organic solids, interplanetary dust particles, and primitive IOM. Variation in functional group concentration amongst these extraterrestrial materials is understood to be a result of various degrees of processing in the parent bodies, in space, during atmospheric entry, etc. These results support the hypothesis that chondritic IOM and cometary refractory organic solids are related chemically and likely were derived from formaldehyde polymer. The fine-scale morphology of formaldehyde polymer produced in the experiment reveals abundant nanospherules that are similar in size and shape to organic nanoglobules that are ubiquitous in primitive chondrites.
C1 [Cody, George D.; Heying, Emily] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Alexander, Conel M. O.; Nittler, Larry R.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Kilcoyne, A. L. David] Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA.
[Sandford, Scott A.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stroud, Rhonda M.] USN, Res Lab, Washington, DC 20015 USA.
RP Cody, GD (reprint author), Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA.
EM gcody@ciw.edu
RI Alexander, Conel/N-7533-2013; Kilcoyne, David/I-1465-2013; Stroud,
Rhonda/C-5503-2008
OI Alexander, Conel/0000-0002-8558-1427; Stroud, Rhonda/0000-0001-5242-8015
FU US Department of Energy; W. M. Keck Foundation; National Science
Foundation; Carnegie Institution of Washington; National Aeronautics and
Space Administration Astrobiology
FX The Advanced Light Source is a US Department of Energy supported
facility. The W. M. Keck Solid State NMR facility at the Geophysical
Laboratory was supported by the W. M. Keck Foundation, the National
Science Foundation, and the Carnegie Institution of Washington. We
gratefully acknowledge support from National Aeronautics and Space
Administration Astrobiology, Origins Program, and Stardust Analysis
programs is gratefully acknowledged.
NR 48
TC 55
Z9 56
U1 3
U2 46
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 NOV 29
PY 2011
VL 108
IS 48
BP 19171
EP 19176
DI 10.1073/pnas.1015913108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 853ZB
UT WOS:000297463100022
PM 21464292
ER
PT J
AU Plante, I
Cucinotta, FA
AF Plante, Ianik
Cucinotta, Francis A.
TI Model of the initiation of signal transduction by ligands in a cell
culture: Simulation of molecules near a plane membrane comprising
receptors
SO PHYSICAL REVIEW E
LA English
DT Article
ID GEMINATE RECOMBINATION; UNIRRADIATED CELLS; BROWNIAN DYNAMICS;
ONE-DIMENSION; AUTOCRINE; INDUCTION; RADIATION; BETA; DIFFUSION;
KINETICS
AB Cell communication is a key mechanism in tissue responses to radiation. Several molecules are implicated in radiation-induced signaling between cells, but their contributions to radiation risk are poorly understood. Meanwhile, Green's functions for diffusion-influenced reactions have appeared in the literature, which are applied to describe the diffusion of molecules near a plane membrane comprising bound receptors with the possibility of reversible binding of a ligand and activation of signal transduction proteins by the ligand-receptor complex. We have developed Brownian dynamics algorithms to simulate particle histories in this system which can accurately reproduce the theoretical distribution of distances of a ligand from the membrane, the number of reversibly bound particles, and the number of receptor complexes activating signaling proteins as a function of time, regardless of the number of time steps used for the simulation. These simulations will be of great importance to model interactions at low doses where stochastic effects induced by a small number of molecules or interactions come into play.
C1 [Plante, Ianik; Cucinotta, Francis A.] NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Plante, Ianik] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
RP Cucinotta, FA (reprint author), NASA Johnson Space Ctr, 2101 NASA Pkwy,Mail Code SK, Houston, TX 77058 USA.
EM Ianik.Plante-1@nasa.gov; Francis.A.Cucinotta@nasa.gov
FU NASA; DoE [DE-AI02-10ER64969]
FX This work was supported by the NASA Space Radiation Risk Assessment
project and the DoE Low Dose Program (DE-AI02-10ER64969). We also thank
Dr. Noam Agmon, Dr. Walter Gautschi, and Dr. Luc Devroye for useful
correspondence.
NR 38
TC 6
Z9 6
U1 0
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1539-3755
J9 PHYS REV E
JI Phys. Rev. E
PD NOV 28
PY 2011
VL 84
IS 5
AR 051920
DI 10.1103/PhysRevE.84.051920
PN 1
PG 13
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA 854BH
UT WOS:000297469000016
PM 22181457
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Belfiore, A
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bottacini, E
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cecchi, C
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
de Angelis, A
de Palma, F
Dermer, CD
Silva, EDE
Drell, PS
Dumora, D
Favuzzi, C
Fegan, SJ
Focke, WB
Fortin, P
Fukazawa, Y
Fusco, P
Gargano, F
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guillemot, L
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hayashi, K
Hays, E
Johannesson, G
Johnson, AS
Kamae, T
Katagiri, H
Kataoka, J
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Martin, P
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pohl, M
Prokhorov, D
Raino, S
Rando, R
Razzano, M
Reposeur, T
Ritz, S
Parkinson, PMS
Sgro, C
Siskind, EJ
Smith, PD
Spinelli, P
Strong, AW
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Tramacere, A
Troja, E
Uchiyama, Y
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Wang, P
Winer, BL
Wood, KS
Yang, Z
Zimmer, S
Bontemps, S
AF Ackermann, M.
Ajello, M.
Allafort, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Belfiore, A.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bottacini, E.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cecchi, C.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
de Angelis, A.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Drell, P. S.
Dumora, D.
Favuzzi, C.
Fegan, S. J.
Focke, W. B.
Fortin, P.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guillemot, L.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hayashi, K.
Hays, E.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Martin, P.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Naumann-Godo, M.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pohl, M.
Prokhorov, D.
Raino, S.
Rando, R.
Razzano, M.
Reposeur, T.
Ritz, S.
Parkinson, P. M. Saz
Sgro, C.
Siskind, E. J.
Smith, P. D.
Spinelli, P.
Strong, A. W.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Tramacere, A.
Troja, E.
Uchiyama, Y.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Zimmer, S.
Bontemps, S.
TI A Cocoon of Freshly Accelerated Cosmic Rays Detected by Fermi in the
Cygnus Superbubble
SO SCIENCE
LA English
DT Article
ID SUPERNOVA REMNANT G78.2+2.1; PARTICLE-ACCELERATION; OB ASSOCIATIONS;
STAR-FORMATION; GAMMA-RAYS; ORIGIN; GALAXY; EMISSION; REGION; DISCOVERY
AB The origin of Galactic cosmic rays is a century-long puzzle. Indirect evidence points to their acceleration by supernova shockwaves, but we know little of their escape from the shock and their evolution through the turbulent medium surrounding massive stars. Gamma rays can probe their spreading through the ambient gas and radiation fields. The Fermi Large Area Telescope (LAT) has observed the star-forming region of Cygnus X. The 1- to 100-gigaelectronvolt images reveal a 50-parsec-wide cocoon of freshly accelerated cosmic rays that flood the cavities carved by the stellar winds and ionization fronts from young stellar clusters. It provides an example to study the youth of cosmic rays in a superbubble environment before they merge into the older Galactic population.
C1 [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.; Tibaldo, L.] Univ Paris Diderot, CEA Saclay, CNRS, CEA IRFU,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Ackermann, M.; Ajello, M.; Allafort, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Orlando, E.; Paneque, D.; Prokhorov, D.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Allafort, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Orlando, E.; Paneque, D.; Prokhorov, D.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; 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.
[Belfiore, A.; Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] IEEE CSIC, Inst Ciencies Espai, Barcelona 08193, Spain.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Ciprini, S.] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Dumora, D.; Lott, B.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guillemot, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Harding, A. K.; Hays, E.; McEnery, J. E.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Johannesson, G.; Troja, E.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] CNRS, Res Inst Astrophys & Planetol IRAP, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Martin, P.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Vitale, V.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Pohl, M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Pohl, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Bontemps, S.] Univ Bordeaux, CNRS, INSU, Lab Astrophys Bordeaux, Floirac, France.
RP Grenier, IA (reprint author), Univ Paris Diderot, CEA Saclay, CNRS, CEA IRFU,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
EM isabelle.grenier@cea.fr; luigi.tibaldo@pd.infn.it
RI Johannesson, Gudlaugur/O-8741-2015; 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;
Hays, Elizabeth/D-3257-2012; Loparco, Francesco/O-8847-2015; Thompson,
David/D-2939-2012; Harding, Alice/D-3160-2012; 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; Tosti, Gino/E-9976-2013;
Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013;
Rando, Riccardo/M-7179-2013
OI Giroletti, Marcello/0000-0002-8657-8852; Tramacere,
Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726;
Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano,
Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Giordano, Francesco/0000-0002-8651-2394; De
Angelis, Alessandro/0000-0002-3288-2517; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214;
SPINELLI, Paolo/0000-0001-6688-8864; Bastieri,
Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018;
Loparco, Francesco/0000-0002-1173-5673; Thompson,
David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806;
giglietto, nicola/0000-0002-9021-2888; Morselli,
Aldo/0000-0002-7704-9553;
FU International Doctorate on Astroparticle Physics (IDAPP) program
FX The Fermi LAT Collaboration acknowledges support from a number of
agencies and institutes for both development and the operation of the
LAT as well as scientific data analysis. These include NASA and the
Department of Energy in the United States; Commissariat a l'Energie
Atomique et aux Energies Alternatives, Institut de Recherche sur les
Lois Fondamentales de l'Univers (CEA/IRFU) and Institut National de
Physique Nucleaire et de Physique des Particules, Centre National de la
Recherche Scientifique (IN2P3/CNRS) in France; Agenzia Spaziale Italiana
(ASI) and Istituto Nazionale di Fisica Nucleare (INFN) in Italy;
Ministry of Education, Culture, Sports, Science, and Technology (MEXT),
Energy Accelerator Research Organization (KEK), and Japan Aerospace
Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation,
Swedish Research Council, and National Space Board in Sweden. Additional
support from Istituto Nazionale di Astrofisica (INAF) in Italy and
Centre National d'Etudes Spaciales (CNES) in France for science analysis
during the operations phase is also gratefully acknowledged. L. T. is
partially supported by the International Doctorate on Astroparticle
Physics (IDAPP) program. E. T is a NASA Postdoctoral Program Fellow.
NR 28
TC 77
Z9 78
U1 0
U2 12
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD NOV 25
PY 2011
VL 334
IS 6059
BP 1103
EP 1107
DI 10.1126/science.1210311
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 852AF
UT WOS:000297313900042
PM 22116880
ER
PT J
AU Freire, PCC
Abdo, AA
Ajello, M
Allafort, A
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Camilo, F
Caraveo, PA
Cecchi, C
Celik, O
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cognard, I
Cohen-Tanugi, J
Cominsky, LR
de Palma, F
Dermer, CD
Silva, EDE
Dormody, M
Drell, PS
Dubois, R
Dumora, D
Espinoza, CM
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Fukazawa, Y
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grondin, MH
Grove, JE
Guillemot, L
Guiriec, S
Hadasch, D
Harding, AK
Johannesson, G
Johnson, AS
Johnson, TJ
Johnston, S
Katagiri, H
Kataoka, J
Keith, M
Kerr, M
Knodlseder, J
Kramer, M
Kuss, M
Lande, J
Latronico, L
Lee, SH
Lemoine-Goumard, M
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Lyne, AG
Manchester, RN
Marelli, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ozaki, M
Paneque, D
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Porter, TA
Raino, S
Ransom, SM
Ray, PS
Reimer, A
Reimer, O
Reposeur, T
Ritz, S
Romani, RW
Roth, M
Sadrozinski, HFW
Parkinson, PMS
Sgro, C
Shannon, R
Siskind, EJ
Smith, DA
Smith, PD
Spinelli, P
Stappers, BW
Suson, DJ
Takahashi, H
Tanaka, T
Tauris, TM
Thayer, JB
Theureau, G
Thompson, DJ
Thorsett, SE
Tibaldo, L
Torres, DF
Tosti, G
Troja, E
Vandenbroucke, J
Van Etten, A
Vasileiou, V
Venter, C
Vianello, G
Vilchez, N
Vitale, V
Waite, AP
Wang, P
Wood, KS
Yang, Z
Ziegler, M
Zimmer, S
AF Freire, P. C. C.
Abdo, A. A.
Ajello, M.
Allafort, A.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Camilo, F.
Caraveo, P. A.
Cecchi, C.
Celik, O.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cognard, I.
Cohen-Tanugi, J.
Cominsky, L. R.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Dormody, M.
Drell, P. S.
Dubois, R.
Dumora, D.
Espinoza, C. M.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grondin, M. -H.
Grove, J. E.
Guillemot, L.
Guiriec, S.
Hadasch, D.
Harding, A. K.
Johannesson, G.
Johnson, A. S.
Johnson, T. J.
Johnston, S.
Katagiri, H.
Kataoka, J.
Keith, M.
Kerr, M.
Knoedlseder, J.
Kramer, M.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Lemoine-Goumard, M.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Lyne, A. G.
Manchester, R. N.
Marelli, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
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.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ozaki, M.
Paneque, D.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Porter, T. A.
Raino, S.
Ransom, S. M.
Ray, P. S.
Reimer, A.
Reimer, O.
Reposeur, T.
Ritz, S.
Romani, R. W.
Roth, M.
Sadrozinski, H. F. -W.
Parkinson, P. M. Saz
Sgro, C.
Shannon, R.
Siskind, E. J.
Smith, D. A.
Smith, P. D.
Spinelli, P.
Stappers, B. W.
Suson, D. J.
Takahashi, H.
Tanaka, T.
Tauris, T. M.
Thayer, J. B.
Theureau, G.
Thompson, D. J.
Thorsett, S. E.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Troja, E.
Vandenbroucke, J.
Van Etten, A.
Vasileiou, V.
Venter, C.
Vianello, G.
Vilchez, N.
Vitale, V.
Waite, A. P.
Wang, P.
Wood, K. S.
Yang, Z.
Ziegler, M.
Zimmer, S.
CA Fermi LAT Collaboration
TI Fermi Detection of a Luminous gamma-Ray Pulsar in a Globular Cluster
SO SCIENCE
LA English
DT Article
ID LARGE-AREA TELESCOPE; MILLISECOND PULSARS; TIMING OBSERVATIONS; RADIO
PULSARS; DISCOVERY; EMISSION; POPULATION; M28
AB We report on the Fermi Large Area Telescope's detection of gamma-ray (>100 mega-electron volts) pulsations from pulsar J1823-3021A in the globular cluster NGC 6624 with high significance (similar to 7 sigma). Its gamma-ray luminosity, L-gamma = (8.4 +/- 1.6) x 10(34) ergs per second, is the highest observed for any millisecond pulsar (MSP) to date, and it accounts for most of the cluster emission. The nondetection of the cluster in the off-pulse phase implies that it contains <32 gamma-ray MSPs, not similar to 100 as previously estimated. The gamma-ray luminosity indicates that the unusually large rate of change of its period is caused by its intrinsic spin-down. This implies that J1823-3021A has the largest magnetic field and is the youngest MSP ever detected and that such anomalous objects might be forming at rates comparable to those of the more normal MSPs.
C1 [Freire, P. C. C.; Guillemot, L.; Kramer, M.; Tauris, T. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Abdo, A. A.; Johnson, T. J.; Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Kerr, M.; Knoedlseder, J.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. B.; Vandenbroucke, J.; Van Etten, A.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Kerr, M.; Knoedlseder, J.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. B.; Vandenbroucke, J.; Van Etten, A.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ballet, J.; Grenier, I. A.; Pierbattista, M.] Univ Paris Diderot, CNRS, CEA IRFU,Serv Astrophys,CEA Saclay, Lab AIM Astrophys Instrumentat & Modelisat, 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.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Sgro, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] IEEE CSIC, Inst Ciencies Espai, Barcelona 08193, Spain.
[Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Caraveo, P. A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Celik, O.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, O.; Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[Celik, O.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, O.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Cheung, C. C.; Johnson, T. J.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Ciprini, S.; Gasparrini, D.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Cognard, I.; Theureau, G.] CNRS, LPCE UMR 6115, Lab Phys & Chem Environm, F-45071 Orleans 02, France.
[Cognard, I.; Theureau, G.] CNRS, INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Ray, P. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Dormody, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Dormody, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Dumora, D.; Lemoine-Goumard, M.; Reposeur, T.; Smith, D. A.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Espinoza, C. M.; Kramer, M.; Lyne, A. G.; Stappers, B. W.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Grondin, M. -H.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Grondin, M. -H.] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Johnston, S.; Keith, M.; Manchester, R. N.; Shannon, R.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.; Vilchez, N.] CNRS, Res Inst Astrophys & Planetol IRAP, F-31028 Toulouse 4, France.
[Vilchez, N.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[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.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Smith, P. D.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Smith, P. D.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem Phys, Hammond, IN 46323 USA.
[Tauris, T. M.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Thorsett, S. E.] Willamette Univ, Dept Phys, Salem, OR 97031 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
RP Freire, PCC (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM pfreire@mpifr-bonn.mpg.de; tyrel.j.johnson@gmail.com;
dmnparent@gmail.com; christo.venter@nwu.ac.za
RI Johannesson, Gudlaugur/O-8741-2015; 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;
Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; Harding,
Alice/D-3160-2012; McEnery, Julie/D-6612-2012; 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; Saz Parkinson, Pablo
Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013; Venter,
Christo/E-6884-2011; Loparco, Francesco/O-8847-2015
OI Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano,
Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Shannon, Ryan/0000-0002-7285-6348; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214;
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;
Venter, Christo/0000-0002-2666-4812; Loparco,
Francesco/0000-0002-1173-5673
FU Science and Technology Facilities Council of the United Kingdom;
European Community [ERC-StG-259391]
FX The Fermi LAT Collaboration acknowledges support from a number of
agencies and institutes for both development and the operation of the
LAT as well as scientific data analysis. These include NASA and the
Department of Energy in the United States; Commissariat a l'Energie
Atomique et aux Energies Alternatives, Institut de Recherche sur les
Lois Fondamentales de l'Univers (CEA/IRFU) and Institut National de
Physique Nucleaire et de Physique des Particules, Centre National de la
Recherche Scientifique (IN2P3/CNRS) in France; Agenzia Spaziale Italiana
(ASI) and Istituto Nazionale di Fisica Nucleare (INFN) in Italy;
Ministry of Education, Culture, Sports, Science, and Technology (MEXT),
Energy Accelerator Research Organization (KEK), and Japan Aerospace
Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation,
Swedish Research Council, and National Space Board in Sweden. Additional
support from Istituto Nazionale di Astrofisica (INAF) in Italy and
Centre National d'Etudes Spaciales (CNES) in France for science analysis
during the operations phase is also gratefully acknowledged. The Nancay
Radio Observatory is operated by the Paris Observatory, associated with
the French CNRS. 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. Fermi LAT data, gamma-ray diffuse models,
and radio pulsar ephemeris are available from the Fermi Science Support
Center (http://fermi.gsfc.nasa.gov/ssc/data/access). M.L.-G. was funded
by contract ERC-StG-259391 from the European Community. E. T. is a NASA
Postdoctoral Program Fellow. We thank the anonymous referees for their
very constructive suggestions.
NR 30
TC 27
Z9 27
U1 2
U2 11
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 NOV 25
PY 2011
VL 334
IS 6059
BP 1107
EP 1110
DI 10.1126/science.1207141
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 852AF
UT WOS:000297313900043
ER
PT J
AU Lawrence, DJ
Eke, VR
Elphic, RC
Feldman, WC
Funsten, HO
Prettyman, TH
Teodoro, LFA
AF Lawrence, David J.
Eke, Vincent R.
Elphic, Richard C.
Feldman, William C.
Funsten, Herbert O.
Prettyman, Thomas H.
Teodoro, Luis F. A.
TI Technical Comment on "Hydrogen Mapping of the Lunar South Pole Using the
LRO Neutron Detector Experiment LEND"
SO SCIENCE
LA English
DT Editorial Material
C1 [Lawrence, David J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Eke, Vincent R.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Teodoro, Luis F. A.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Feldman, William C.; Prettyman, Thomas H.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Funsten, Herbert O.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Lawrence, DJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM david.j.lawrence@jhuapl.edu
RI Funsten, Herbert/A-5702-2015; Lawrence, David/E-7463-2015;
OI Funsten, Herbert/0000-0002-6817-1039; Lawrence,
David/0000-0002-7696-6667; Prettyman, Thomas/0000-0003-0072-2831
NR 9
TC 15
Z9 15
U1 1
U2 7
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 NOV 25
PY 2011
VL 334
IS 6059
DI 10.1126/science.1203341
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 852AF
UT WOS:000297313900027
PM 22116865
ER
PT J
AU Iarve, EV
Gurvich, MR
Mollenhauer, DH
Rose, CA
Davila, CG
AF Iarve, Endel V.
Gurvich, Mark R.
Mollenhauer, David H.
Rose, Cheryl A.
Davila, Carlos G.
TI Mesh-independent matrix cracking and delamination modeling in laminated
composites
SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN ENGINEERING
LA English
DT Article
DE composite; mesh independent cracking; delamination; failure
ID FINITE-ELEMENT-METHOD; CONTINUUM DAMAGE MODEL; PART I; DISCONTINUITIES;
MICROMECHANICS; SIMULATION; SPECIMENS; FAILURE; LAW
AB The initiation and evolution of transverse matrix cracks and delaminations are predicted within a mesh-independent cracking (MIC) framework. MIC is a regularized extended finite element method (x-FEM) that allows the insertion of cracks in directions that are independent of the mesh orientation. The Heaviside step function that is typically used to introduce a displacement discontinuity across a crack surface is replaced by a continuous function approximated by using the original displacement shape functions. Such regularization allows the preservation of the Gaussian integration schema regardless of the enrichment required to model cracking in an arbitrary direction. The interaction between plies is anchored on the integration point distribution, which remains constant through the entire simulation. Initiation and propagation of delaminations between plies as well as intra-ply MIC opening is implemented by using a mixed-mode cohesive formulation in a fully three-dimensional model that includes residual thermal stresses. The validity of the proposed methodology was tested against a variety of problems ranging from simple evolution of delamination from existing transverse cracks to strength predictions of complex laminates without a priori knowledge of damage location or initiation. Good agreement with conventional numerical solutions and/or experimental data was observed in all the problems considered. Published 2011. This article is a US Government work and is in the public domain in the USA.
C1 [Iarve, Endel V.; Mollenhauer, David H.] USAF, Res Lab, Wright Patterson AFB, OH 45433 USA.
[Iarve, Endel V.] Univ Dayton, Res Inst, Dayton, OH 45469 USA.
[Gurvich, Mark R.] United Technol Res Ctr, E Hartford, CT 06108 USA.
[Rose, Cheryl A.; Davila, Carlos G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Iarve, EV (reprint author), USAF, Res Lab, 2941 Hobson Way, Wright Patterson AFB, OH 45433 USA.
EM endel.iarve@wpafb.af.mil
RI Davila, Carlos/D-8559-2011
FU NASA AAD-2 [NNX08AB05A-G]; AFRL [FA8650-05-D-5052]; University of Dayton
Research Institute
FX The work was funded under NASA AAD-2 contract number NNX08AB05A-G and
partially by AFRL contract FA8650-05-D-5052 with the University of
Dayton Research Institute.
NR 36
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U1 3
U2 27
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0029-5981
J9 INT J NUMER METH ENG
JI Int. J. Numer. Methods Eng.
PD NOV 25
PY 2011
VL 88
IS 8
BP 749
EP 773
DI 10.1002/nme.3195
PG 25
WC Engineering, Multidisciplinary; Mathematics, Interdisciplinary
Applications
SC Engineering; Mathematics
GA 847YR
UT WOS:000297012500002
ER
PT J
AU Katsuda, S
Mori, K
Petre, R
Yamaguchi, H
Tsunemi, H
Bocchino, F
Bamba, A
Miceli, M
Hewitt, JW
Temim, T
Uchida, H
Yoshii, R
AF Katsuda, Satoru
Mori, Koji
Petre, Robert
Yamaguchi, Hiroya
Tsunemi, Hiroshi
Bocchino, Fabrizio
Bamba, Aya
Miceli, Marco
Hewitt, John W.
Temim, Tea
Uchida, Hiroyuki
Yoshii, Rie
TI Suzaku Detection of Diffuse Hard X-Ray Emission outside Vela X
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE ISM: individual (Vela Pulsar Wind Nebula); ISM: supernova remnants;
X-rays: ISM
ID PULSAR WIND NEBULAE; SHOCK-CLOUD INTERACTION; ROSAT PSPC OBSERVATION;
SUPERNOVA REMNANT; SPECTRAL-ANALYSIS; RX J0852.0-4622; SHRAPNEL-A; HESS;
SPECTROSCOPY; REGION
AB Vela X is a large, 3 degrees x 2 degrees, radio-emitting pulsar wind nebula (PWN) powered by the Vela pulsar in the Vela supernova remnant. Using four Suzaku/XIS observations pointed just outside Vela X, we have found hard X-ray emission extending throughout the fields of view. The hard X-ray spectra are well represented by a power-law. The photon index was measured to be constant at Gamma similar to 2.4, similar to that of the southern outer part of Vela X. The power-law flux decreases with increasing distance from the pulsar. These properties lead us to propose that the hard X-ray emission is associated with the Vela PWN. The larger X-ray extension found in this work strongly suggests that distinct populations of relativistic electrons form the X-ray PWN and Vela X, as was recently inferred from multiwavelength spectral modeling of Vela X.
C1 [Katsuda, Satoru; Yamaguchi, Hiroya; Yoshii, Rie] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan.
[Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys, Miyazaki 8892192, Japan.
[Tsunemi, Hiroshi; Uchida, Hiroyuki] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Bocchino, Fabrizio; Miceli, Marco] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy.
[Bamba, Aya] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland.
[Bamba, Aya] ISAS JAXA Dept High Energy Astrophys, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Miceli, Marco] Univ Palermo, Sez Astron, Dipartimento Sci Fis & Astron, I-90134 Palermo, Italy.
[Katsuda, Satoru; Petre, Robert; Hewitt, John W.; Temim, Tea] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Katsuda, S (reprint author), RIKEN, Inst Phys & Chem Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.
EM katsuda@crab.riken.jp
RI XRAY, SUZAKU/A-1808-2009;
OI Miceli, Marco/0000-0003-0876-8391; Temim, Tea/0000-0001-7380-3144
FU JSPS; NASA [NNG06EO90A]
FX We would like to express our special thanks to Una Hwang for a number of
useful comments, and Douglas Bock and the HESS collaboration for
providing a radio (843 MHz) image and a HESS image of Vela X,
respectively. S.K. is supported by a JSPS Research Fellowship for
Research Abroad, and in part by the NASA grant under the contract
NNG06EO90A.
NR 48
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U1 0
U2 0
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 NOV 25
PY 2011
VL 63
SI 3
BP S827
EP S836
DI 10.1093/pasj/63.sp3.S827
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 877OM
UT WOS:000299191800020
ER
PT J
AU Saitou, K
Tsujimoto, M
Ebisawa, K
Ishida, M
Mukai, K
Nagayama, T
Nishiyama, S
Gandhi, P
AF Saitou, Kei
Tsujimoto, Masahiro
Ebisawa, Ken
Ishida, Manabu
Mukai, Koji
Nagayama, Takahiro
Nishiyama, Shogo
Gandhi, Poshak
TI Near-Infrared and X-Ray Observations of XSS J12270-4859
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE infrared: stars; stars: individual (XSS J12270-4859); stars: variables:
other; X-rays: stars
ID ALL-SKY SURVEY; SYNCHROTRON EMISSION; OPTICAL VARIABILITY;
INTERSTELLAR-MEDIUM; SURVEY CATALOG; XTE J1118+480; GRS 1915+105;
BLACK-HOLE; GX 339-4; JET
AB XSS J12270-4859 (J12270) is an enigmatic source of unknown nature. Previous studies revealed that the source has unusual X-ray temporal characteristics, including repetitive short-term flares, followed by spectral hardening, non-periodic dips, and dichotomy in activity; i.e., intervals filled with flares and those without. Together with a power-law X-ray spectrum, it is suggested to be a low-mass X-ray binary. In order to better understand the object, we present the results of our near-infrared (NIR) photometry and linear polarimetry observations as well as X-ray spectroscopy observations, which overlap with each other partially in time, taken respectively with the InfraRed Survey Facility (IRSF) and the Rossi X-ray Tinting Explorer (RXTE). We detected several simultaneous NIR and X-ray flares for the first time. No significant NIR polarization was obtained. We assembled data taken with IRSF, RXTE, Suzaku, Swift, and other missions in the literature and compared the flare profile and the spectral energy distribution (SED) with some representative high-energy sources. Based on some similarities of the repetitive NIR and X-ray flaring characteristics and the broad SED, we argue that J12270 is reminiscent of microquasars with a synchrotron jet, which is at a very low-luminosity state of approximate to 10(-4) Eddington luminosity for a stellar mass black hole or neutron star at a reference distance of 1 kpc.
C1 [Saitou, Kei; Tsujimoto, Masahiro; Ebisawa, Ken; Ishida, Manabu; Gandhi, Poshak] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Saitou, Kei; Ebisawa, Ken] Univ Tokyo, Dept Astron, Grad Sch Sci, Bunkyo Ku, Tokyo 1130033, Japan.
[Mukai, Koji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nagayama, Takahiro] Nagoya Univ, Grad Sch Sci, Dept Phys, Nagoya, Aichi 4648602, Japan.
[Nishiyama, Shogo] Natl Inst Nat Sci, Natl Astron Observ Japan, Extrasolar Planet Detect Project Off, Mitaka, Tokyo 1818588, Japan.
RP Saitou, K (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
EM ksaitou@astro.isas.jaxa.jp
RI XRAY, SUZAKU/A-1808-2009
FU Japan Society for the Promotion of Science; Hayakawa foundation of the
Astronomical Society of Japan
FX We thank Daisuke Kato for his help in obtaining NIR data for a SIRIUS
run, Hirofumi Hatano for advice in polarimetry data reduction, Shinki
Oyabu for advice on the AKARI survey data, and Hajime Inoue and Mamoru
Doi for useful discussion. We appreciate the telescope managers of RXTE
for allocating telescope time for our observations. K. S. is financially
supported by Japan Society for the Promotion of Science and the Hayakawa
foundation of the Astronomical Society of Japan.
NR 52
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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 NOV 25
PY 2011
VL 63
SI 3
BP S759
EP S769
DI 10.1093/pasj/63.sp3.S759
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 877OM
UT WOS:000299191800014
ER
PT J
AU Shidatsu, M
Ueda, Y
Tazaki, F
Yoshikawa, T
Nagayama, T
Nagata, T
Oi, N
Yamaoka, K
Takahashi, H
Kubota, A
Cottam, J
Remillard, R
Negoro, H
AF Shidatsu, Megumi
Ueda, Yoshihiro
Tazaki, Fumie
Yoshikawa, Tatsuhito
Nagayama, Takahiro
Nagata, Tetsuya
Oi, Nagisa
Yamaoka, Kazutaka
Takahashi, Hiromitsu
Kubota, Aya
Cottam, Jean
Remillard, Ronald
Negoro, Hitoshi
TI X-Ray and Near-Infrared Observations of GX 339-4 in the Low/Hard State
with Suzaku and IRSF
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE accretion, accretion disks; black hole physics; infrared: stars; stars:
individual (GX 339-4); X-rays: binaries
ID ACCRETING BLACK-HOLES; TIMING OBSERVATIONS; COMPACT JET; HARD STATE;
RADIO JET; GX-339-4; BINARIES; EMISSION; SPECTRA; SPIN
AB X-ray and near-infrared (J-H-K-s) observations of the galactic black-hole binary GX 339-4 in the low/hard state were performed with Suzaku and IRSF in 2009 March. The spectrum in the 0.5-300 keV band is dominated by thermal Comptonization of multicolor disk photons, with a small contribution from a direct disk component, indicating that the inner disk is almost fully covered by hot corona with an electron temperature of approximate to 175 keV. The Comptonizing corona has at least two optical depths, tau approximate to 1, 0.4. Analysis of the iron-K line profile yields an inner-disk radius of (13.3(-6.0)(+6.04)) R-g (R-g represents the gravitational radius GM/c(2)), with the best-fit inclination angle of approximate to 50 degrees. This radius is consistent with that estimated from the continuum fit by assuming the conservation of photon numbers in Comptonization. Our results suggest that the standard disk of GX 339-4 is likely truncated before reaching the innermost stable circular orbit (for a non-rotating black hole) in the low/hard states at similar to 1% of the Eddington luminosity. The one-day averaged near-infrared light curves are found to be correlated with hard X-ray flux with F-Ks proportional to F-X(0.45). The flatter near-infrared vF(v) spectrum than the radio one suggests that the optically thin synchrotron radiation from the compact jets dominates the near-infrared flux. Based on a simple analysis, we estimate the magnetic field and size of the jet base to be 5 x 10(4) G and 6 x 10(8) cm, respectively. The synchrotron self Compton component is estimated to be approximately 0.4% of the total X-ray flux.
C1 [Shidatsu, Megumi; Ueda, Yoshihiro; Tazaki, Fumie; Yoshikawa, Tatsuhito; Nagata, Tetsuya] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Nagayama, Takahiro] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Oi, Nagisa] Grad Univ Adv Studies, Dept Astron, Mitaka, Tokyo 1818588, Japan.
[Yamaoka, Kazutaka] Aoyama Gakuin Univ, Dept Phys, Chuo Ku, Sagamihara, Kanagawa 2298558, Japan.
[Takahashi, Hiromitsu] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Kubota, Aya] Shibaura Inst Technol, Dept Elect Informat Syst, Minuma Ku, Saitama 3378570, Japan.
[Cottam, Jean] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA.
[Remillard, Ronald] MIT, Dept Phys, Cambridge, MA 02138 USA.
[Negoro, Hitoshi] Nihon Univ, Dept Phys, Chiyoda Ku, Tokyo 1018308, Japan.
RP Shidatsu, M (reprint author), Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
EM shidatsu@kusastro.kyoto-u.ac.jp; ueda@kusastro.kyoto-u.ac.jp
RI XRAY, SUZAKU/A-1808-2009; Shidatsu, Megumi/C-5742-2017
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) of
Japan [20540230]; Global COE, Ministry of Education, Culture, Sports,
Science and Technology (MEXT) of Japan
FX This work was partly supported by a Grant-in-Aid for Scientific
Research, 20540230 (YU), and by a grant-in-aid for the Global COE
Program "The Next Generation of Physics, Spun from Universality and
Emergence" from the Ministry of Education, Culture, Sports, Science and
Technology (MEXT) of Japan. We are grateful to the Suzaku operation team
for carrying out the ToO observations.
NR 59
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U2 0
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 NOV 25
PY 2011
VL 63
SI 3
BP S785
EP S801
DI 10.1093/pasj/63.sp3.S785
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 877OM
UT WOS:000299191800016
ER
PT J
AU van Dijk, AIJM
Renzullo, LJ
Rodell, M
AF van Dijk, A. I. J. M.
Renzullo, L. J.
Rodell, M.
TI Use of Gravity Recovery and Climate Experiment terrestrial water storage
retrievals to evaluate model estimates by the Australian water resources
assessment system
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID SATELLITE ALTIMETRY; GRACE; SURFACE; ASSIMILATION; BUDGET; EARTH
AB Terrestrial water storage (TWS) estimates retrieved from the Gravity Recovery and Climate Experiment (GRACE) satellite mission were compared to TWS modeled by the Australian Water Resources Assessment (AWRA) system. The aim was to test whether differences could be attributed and used to identify model deficiencies. Data for 2003-2010 were decomposed into the seasonal cycle, linear trends and the remaining de-trended anomalies before comparing. AWRA tended to have smaller seasonal amplitude than GRACE. GRACE showed a strong (>15 mm yr(-1)) drying trend in northwest Australia that was associated with a preceding period of unusually wet conditions, whereas weaker drying trends in the southern Murray Basin and southwest Western Australia were associated with relatively dry conditions. AWRA estimated trends were less negative for these regions, while a more positive trend was estimated for areas affected by cyclone Charlotte in 2009. For 2003-2009, a decrease of 7-8 mm yr(-1) (50-60 km(3) yr(-1)) was estimated from GRACE, enough to explain 6%-7% of the contemporary rate of global sea level rise. This trend was not reproduced by the model. Agreement between model and data suggested that the GRACE retrieval error estimates are biased high. A scaling coefficient applied to GRACE TWS to reduce the effect of signal leakage appeared to degrade quantitative agreement for some regions. Model aspects identified for improvement included a need for better estimation of rainfall in northwest Australia, and more sophisticated treatment of diffuse groundwater discharge processes and surface-groundwater connectivity for some regions.
C1 [van Dijk, A. I. J. M.; Renzullo, L. J.] CSIRO Land & Water, Black Mt Labs, Canberra, ACT 2601, Australia.
[Rodell, M.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP van Dijk, AIJM (reprint author), CSIRO Land & Water, Black Mt Labs, Canberra, ACT 2601, Australia.
EM albert.vandijk@csiro.au
RI Rodell, Matthew/E-4946-2012; Renzullo, Luigi/D-5797-2011; Van Dijk,
Albert/B-3106-2011
OI Rodell, Matthew/0000-0003-0106-7437; Renzullo,
Luigi/0000-0003-3056-4109; Van Dijk, Albert/0000-0002-6508-7480
FU NASA
FX This work is part of the water information research and development
alliance between the Bureau of Meteorology and CSIRO's Water for a
Healthy Country Flagship. GRACE land data were processed by Sean
Swenson, supported by the NASA MEASURES Program, and are available at
http://grace.jpl.nasa.gov. Helpful suggestions from Paul Tregoning, Sean
Swenson, Richard Cresswell, Glenn Harrington, Brian Smerdon, Don
McFarlane, Tom van Niel and John Church are gratefully acknowledged.
NR 33
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U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
J9 WATER RESOUR RES
JI Water Resour. Res.
PD NOV 24
PY 2011
VL 47
AR W11524
DI 10.1029/2011WR010714
PG 12
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 853IR
UT WOS:000297419900001
ER
PT J
AU Noone, D
Galewsky, J
Sharp, ZD
Worden, J
Barnes, J
Baer, D
Bailey, A
Brown, DP
Christensen, L
Crosson, E
Dong, F
Hurley, JV
Johnson, LR
Strong, M
Toohey, D
Van Pelt, A
Wright, JS
AF Noone, David
Galewsky, Joseph
Sharp, Zachary D.
Worden, John
Barnes, John
Baer, Doug
Bailey, Adriana
Brown, Derek P.
Christensen, Lance
Crosson, Eric
Dong, Feng
Hurley, John V.
Johnson, Leah R.
Strong, Mel
Toohey, Darin
Van Pelt, Aaron
Wright, Jonathon S.
TI Properties of air mass mixing and humidity in the subtropics from
measurements of the D/H isotope ratio of water vapor at the Mauna Loa
Observatory
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LARGE-SCALE ADVECTION; BOUNDARY-LAYER; CARBON-DIOXIDE; CLOUD;
CONVECTION; CLIMATE; HAWAII; CYCLE; MAINTENANCE; TROPOSPHERE
AB Water vapor in the subtropical troposphere plays an important role in the radiative balance, the distribution of precipitation, and the chemistry of the Earth's atmosphere. Measurements of the water vapor mixing ratio paired with stable isotope ratios provide unique information on transport processes and moisture sources that is not available with mixing ratio data alone. Measurements of the D/H isotope ratio of water vapor from Mauna Loa Observatory over 4 weeks in October-November 2008 were used to identify components of the regional hydrological cycle. A mixing model exploits the isotope information to identify water fluxes from time series data. Mixing is associated with exchange between marine boundary layer air and tropospheric air on diurnal time scales and between different tropospheric air masses with characteristics that evolve on the synoptic time scale. Diurnal variations are associated with upslope flow and the transition from nighttime air above the marine trade inversion to marine boundary layer air during daytime. During easterly trade wind conditions, growth and decay of the boundary layer are largely conservative in a regional context but contribute similar to 12% of the nighttime water vapor at Mauna Loa. Tropospheric moisture is associated with convective outflow and exchange with drier air originating from higher latitude or higher altitude. During the passage of a moist filament, boundary layer exchange is enhanced. Isotopic data reflect the combination of processes that control the water balance, which highlights the utility for baseline measurements of water vapor isotopologues in monitoring the response of the hydrological cycle to climate change.
C1 [Noone, David; Bailey, Adriana; Brown, Derek P.; Toohey, Darin] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Noone, David; Bailey, Adriana; Brown, Derek P.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Galewsky, Joseph; Sharp, Zachary D.; Hurley, John V.; Johnson, Leah R.; Strong, Mel] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Worden, John; Christensen, Lance] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Barnes, John] Natl Atmospher & Ocean Adm, Mauna Loa Observ, Hilo, HI 96720 USA.
[Baer, Doug; Dong, Feng] Los Gatos Res Inc, Mountain View, CA 94041 USA.
[Crosson, Eric; Van Pelt, Aaron] Picarro Inc, Santa Clara, CA 95054 USA.
[Wright, Jonathon S.] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB4 1EN, England.
RP Noone, D (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, Campus Box 216, Boulder, CO 80309 USA.
EM dcn@colorado.edu
RI Toohey, Darin/A-4267-2008; hurley, john/A-8707-2015; Bailey,
Adriana/J-2066-2015;
OI Toohey, Darin/0000-0003-2853-1068; Bailey, Adriana/0000-0002-2614-1560;
Wright, Jonathon/0000-0001-6551-7017
FU National Science Foundation [0840129, 0840168]; NASA Jet Propulsion
Laboratory
FX This work was supported by the National Science Foundation Climate and
Large-scale Dynamics program under grants 0840129 and 0840168 to D.N.,
J.G., and Z.D.S. and by the NASA Jet Propulsion Laboratory. We thank all
the staff at Mauna Loa Observatory and the NOAA office in Hilo who
helped with logistics and daily operations during the field campaign.
Isotope ratio data from this study are available in raw and calibrated
form from http://climate.colorado.edu/research/HAVAIKI.
NR 73
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U1 1
U2 27
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 NOV 23
PY 2011
VL 116
AR D22113
DI 10.1029/2011JD015773
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 853JF
UT WOS:000297421400001
ER
PT J
AU Carton, JA
Chepurin, GA
Reagan, J
Hakkinen, S
AF Carton, James A.
Chepurin, Gennady A.
Reagan, James
Haekkinen, Sirpa
TI Interannual to decadal variability of Atlantic Water in the Nordic and
adjacent seas
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID NORTHERN NORTH-ATLANTIC; WEST SPITSBERGEN CURRENT; ARCTIC-OCEAN; BARENTS
SEA; SURFACE-TEMPERATURE; FRAM STRAIT; INFLOW; HYDROGRAPHY; CIRCULATION;
REANALYSIS
AB Warm salty Atlantic Water is the main source water for the Arctic Ocean and thus plays an important role in the mass and heat budget of the Arctic. This study explores interannual to decadal variability of Atlantic Water properties in the Nordic Seas area where Atlantic Water enters the Arctic, based on a reexamination of the historical hydrographic record for the years 1950-2009, obtained by combining multiple data sets. The analysis shows a succession of four multiyear warm events where temperature anomalies at 100 m depth exceed 0.4 degrees C, and three cold events. Three of the four warm events lasted 3-4 years, while the fourth began in 1999 and persists at least through 2009. This most recent warm event is anomalous in other ways as well, being the strongest, having the broadest geographic extent, being surface-intensified, and occurring under exceptional meteorological conditions. Three of the four warm events were accompanied by elevated salinities consistent with enhanced ocean transport into the Nordic Seas, with the exception of the event spanning July 1989-July 1993. Of the three cold events, two lasted for 4 years, while the third lasted for nearly 14 years. Two of the three cold events are associated with reduced salinities, but the cold event of the 1960s had elevated salinities. The relationship of these events to meteorological conditions is examined. The results show that local surface heat flux variations act in some cases to reinforce the anomalies, but are too weak to be the sole cause.
C1 [Carton, James A.; Chepurin, Gennady A.; Reagan, James] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20743 USA.
[Haekkinen, Sirpa] NASA, Goddard Space Flight Ctr, Ice Branch, Greenbelt, MD 20771 USA.
RP Carton, JA (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, Comp & Space Sci Bldg, College Pk, MD 20743 USA.
EM carton@atmos.umd.edu
RI Hakkinen, Sirpa/E-1461-2012; carton, james/C-4807-2009
OI carton, james/0000-0003-0598-5198
FU National Science Foundation [OCE0752209]; NASA
FX We are grateful to the NOAA Earth System Research Laboratory, Physical
Sciences Division for access to their High Resolution SST data,
(www.esrl.noaa.gov/psd/), to the NOAA National Oceanographic Data Center
(www.nodc.noaa.gov), the International Council of the Exploration of the
Seas (www.ices.dk), the Woods Hole Oceanographic Institution
Ice-Tethered Profile (www.whoi.edu/page.do?pid = 20781) and Hydrobase II
(www.whoi.edu/science/PO/hydrobase/) archives for providing access to
their hydrographic data sets. Without their cooperation this work would
not be possible. The anonymous reviewers significantly improved this
manuscript. JAC, JR, and GAC gratefully acknowledge support by the
National Science Foundation (OCE0752209). SH gratefully acknowledges the
support of the NASA OSTM Physical Oceanography Program.
NR 54
TC 16
Z9 16
U1 0
U2 17
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 NOV 23
PY 2011
VL 116
AR C11035
DI 10.1029/2011JC007102
PG 13
WC Oceanography
SC Oceanography
GA 853JP
UT WOS:000297422400001
ER
PT J
AU Kuttippurath, J
Kleinbohl, A
Sinnhuber, M
Bremer, H
Kullmann, H
Notholt, J
Godin-Beekmann, S
Tripathi, O
Nikulin, G
AF Kuttippurath, Jayanarayanan
Kleinboehl, Armin
Sinnhuber, Miriam
Bremer, Holger
Kuellmann, Harry
Notholt, Justus
Godin-Beekmann, Sophie
Tripathi, Omprakash
Nikulin, Grigory
TI Arctic ozone depletion in 2002-2003 measured by ASUR and comparison with
POAM observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID POLAR STRATOSPHERIC CLOUDS; WINTER 2002/2003; CHLORINE ACTIVATION;
SUBMILLIMETER RADIOMETER; 3-DIMENSIONAL MODEL; VORTEX; TRANSPORT;
DENITRIFICATION; VARIABILITY; SIMULATION
AB We present ozone loss estimated from airborne measurements taken during January-February and March in the Arctic winter 2002/2003. The first half of the winter was characterized by unusually cold temperatures and the second half by a major stratospheric sudden warming around 15-18 January 2003. The potential vorticity maps show a vortex split in the lower stratosphere during the major warming (MW) in late January and during the minor warming in mid-February due to wave 1 amplification. However, the warming can be termed as a vortex displacement event as there was no vortex split during the MW period at 10 hPa. Very low temperatures, large areas of polar stratospheric clouds (PSCs), and high chlorine activation triggered significant ozone loss in the early winter, as the vortex moved to the midlatitude regions. The ozone depletion derived from the ASUR measurements sampled inside the vortex, in conjunction with the Mimosa-Chim model tracer, shows a maximum of 1.3 +/- 0.2 ppmv at 450-500 K by late March. The partial column loss derived from the ASUR ozone profiles reaches up to 61 +/- 4 DU in 400-550 K in the same period. The evolution of ozone and ozone loss assessed from the ASUR measurements is in very good agreement with POAM observations. The reduction in ozone estimated from the POAM measurements shows a similar maximum of 1.3 +/- 0.2 ppmv at 400-500 K or 63 +/- 4 DU in 400-550 K in late March. Our study reveals that the Arctic winter 2002/2003 was unique as it had three minor warmings and a MW, yet showed large loss in ozone. No such feature was observed in any other Arctic winter in the 1989-2010 period. In addition, an unusually large ozone loss in December, around 0.5 +/- 0.2 ppmv at 450-500 K or 12 +/- 1 DU in 400-550 K, was estimated for the first time in the Arctic. A careful and detailed diagnosis with all available published results for this winter exhibits an average ozone loss of 1.5 +/- 0.3 ppmv at 450-500 K or 65 +/- 5 DU in 400-550 K by the end of March, which exactly matches the ozone depletion derived from the ASUR, POAM and model data. The early ozone loss together with considerable loss afterwards put the warm Arctic winter 2002/2003 amongst the moderately cold winters in terms of the significance of the ozone loss.
C1 [Kuttippurath, Jayanarayanan; Sinnhuber, Miriam; Bremer, Holger; Kuellmann, Harry; Notholt, Justus] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany.
[Kuttippurath, Jayanarayanan; Godin-Beekmann, Sophie] UPMC, LATMOS, CNRS, F-75005 Paris, France.
[Kleinboehl, Armin] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sinnhuber, Miriam] Karlsruhe Inst Technol, IMK, D-76131 Karlsruhe, Germany.
[Bremer, Holger] Phys Tech Bundensanstalt, Braunschweig, Germany.
[Tripathi, Omprakash] Univ Arizona, Dept Atmospher Sci, Tucson, AZ 85721 USA.
[Nikulin, Grigory] Swedish Meteorol & Hydrol Inst, Rossby Ctr, SE-60176 Norrkoping, Sweden.
RP Kuttippurath, J (reprint author), Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany.
EM jayan@aero.jussieu.fr
RI Sinnhuber, Miriam/A-7252-2013; Notholt, Justus/P-4520-2016
OI Notholt, Justus/0000-0002-3324-885X
FU German contribution [FKZ 50EE 0022]; ESA [349]
FX We thank Gunter Naveke for his assistance with the ASUR radiometer
operation prior to the campaigns. The ECMWF data are taken from the
NILU/NADIR CALVAL database. We thank Karl Hoppel and the POAM team at
the US Naval Research Laboratory for providing the POAM data
(http:wvms.nrl.navy.mil:/POAM/). We also thank the EuPLEx and SCIA-VALUE
2003 project teams for making available ASUR on-board the DLR-Falcon 20
aircraft to perform the trace gas observations. The project was funded
by the German contribution to the ENVISAT validation under the contract
FKZ 50EE 0022 and was a part of the ESA proposal A.O.ID 349.
NR 53
TC 3
Z9 3
U1 0
U2 6
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 NOV 22
PY 2011
VL 116
AR D22305
DI 10.1029/2011JD016020
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 853JD
UT WOS:000297421100001
ER
PT J
AU Miller, DJ
Sun, K
Zondlo, MA
Kanter, D
Dubovik, O
Welton, EJ
Winker, DM
Ginoux, P
AF Miller, David J.
Sun, Kang
Zondlo, Mark A.
Kanter, David
Dubovik, Oleg
Welton, Ellsworth Judd
Winker, David M.
Ginoux, Paul
TI Assessing boreal forest fire smoke aerosol impacts on U.S. air quality:
A case study using multiple data sets
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BIOMASS BURNING EMISSIONS; SKY RADIANCE MEASUREMENTS; LONG-RANGE
TRANSPORT; OPTICAL-PROPERTIES; UNITED-STATES; CARBON-MONOXIDE; BLACK
CARBON; PLUMES; CANADA; LIDAR
AB We synthesize multiple ground-based and satellite measurements to track the physical and chemical evolution of biomass burning smoke plumes transported from western Canada to the northeastern U.S. This multiple data set case study is an advantageous methodology compared with using individual or small groups of data sets, each with their own limitations. The case study analyzed is a Canadian boreal forest fire event on July 4, 2006 with carbonaceous aerosol smoke emission magnitudes comparable to those during the summer fire seasons of the previous decade. We track long-range transport of these aerosol plumes with data from space-borne remote sensing satellite instruments (MODIS, OMI, MISR, CALIOP lidar, AIRS) and ground-based in situ and remote aerosol observations (AERONET CIMEL sky/Sun photometer, MPLNET lidar, IMPROVE, EPA AirNow). Convective lofting elevated smoke emissions above the boundary layer into the free troposphere, where high speed winds aloft led to rapid, long-range transport. Aerosol layer subsidence occurred during transport due to a region of surface high pressure. Smoke aerosols reaching the boundary layer led to surface fine particulate matter (PM2.5) enhancements accompanied by changes in aerosol composition as the plume mixed with anthropogenic aerosols over the northeastern U.S. The extensive coverage of this smoke plume over the northeastern U.S. affected regional air quality, with increases of 10-20 mu g m(-3) PM2.5 attributable to biomass burning smoke aerosols and EPA 24-hour PM2.5 standard exceedances along the U.S. East Coast. Although each data set individually provides a limited view of the transport of smoke emissions, we demonstrate that a multi-data set approach results in a more comprehensive view of potential impacts due to long-range transport of smoke from a less extreme fire event. Our case study demonstrates that fires emit smoke aerosols that under certain meteorological conditions can degrade regional air quality 3000 km from the source region, with additional implications for aerosol radiative forcing and regional haze over the northeastern U.S.
C1 [Miller, David J.; Sun, Kang; Zondlo, Mark A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Kanter, David] Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA.
[Dubovik, Oleg] Univ Lille 1, CNRS, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France.
[Welton, Ellsworth Judd] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Ginoux, Paul] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA.
RP Miller, DJ (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
EM djmtwo@princeton.edu; kangsun@princeton.edu; mzondlo@princeton.edu;
dkanter@princeton.edu; dubovik@loa.univ-lille1.fr;
ellsworth.j.welton@nasa.gov; david.m.winker@nasa.gov;
Paul.Ginoux@noaa.gov
RI Dubovik, Oleg/A-8235-2009; Xiongfei, Zhao/G-7690-2015; Zondlo,
Mark/R-6173-2016; Welton, Ellsworth/A-8362-2012; Ginoux,
Paul/C-2326-2008
OI Dubovik, Oleg/0000-0003-3482-6460; Zondlo, Mark/0000-0003-2302-9554;
Ginoux, Paul/0000-0003-3642-2988
FU NASA; National Science Foundation
FX We wish to thank the developers of the AERONET Data Synergy Tool and
GIOVANNI online data system (developed and maintained by NASA GES DISC)
which greatly facilitated the extraction of visualizations of MODIS,
MISR, AERONET, MPLNET, back trajectories, EPA AirNOW and AIRS CO column
data. We would like to acknowledge Ralph Kahn, who provided invaluable
insights, David Nelson for the MISR-MINX plume height database, Omar
Torres for the availability of OMI AI data, and Brent Holben for AERONET
data availability. Data from the Pickle Lake AERONET site are provided
by the Canadian network AEROCAN, part of NASA's AERONET federated
networks. COVE site data are funded by the NASA Earth Observing System
project and MPLNET is funded by the NASA Earth Observing System and
Radiation Sciences Program. We also greatly appreciate the use of the
USDA fire maps, CALIOP, IMPROVE and NCEP data as well as the NOAA
HYSPLIT trajectory computations. David J. Miller is supported by a
Graduate Research Fellowship from the National Science Foundation.
NR 59
TC 10
Z9 10
U1 2
U2 24
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD NOV 22
PY 2011
VL 116
AR D22209
DI 10.1029/2011JD016170
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 853JD
UT WOS:000297421100003
ER
PT J
AU Yokoyama, T
Yamamoto, M
Otsuka, Y
Nishioka, M
Tsugawa, T
Watanabe, S
Pfaff, RF
AF Yokoyama, T.
Yamamoto, M.
Otsuka, Y.
Nishioka, M.
Tsugawa, T.
Watanabe, S.
Pfaff, R. F.
TI On postmidnight low-latitude ionospheric irregularities during solar
minimum: 1. Equatorial Atmosphere Radar and GPS-TEC observations in
Indonesia
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID FIELD-ALIGNED IRREGULARITIES; REGION PLASMA DRIFTS; SPREAD-F;
MIDLATITUDE IONOSPHERE; MU RADAR; PEDERSEN CONDUCTIVITY;
GEOMAGNETIC-ACTIVITY; THERMOSPHERIC WINDS; DISTURBANCES; INSTABILITY
AB Using the 47 MHz Equatorial Atmosphere Radar (EAR) in West Sumatra, Indonesia (10.36 degrees S dip latitude), it is shown that postmidnight irregularities during solar minimum are morphologically different from those detected during solar maximum and are quite similar to those observed with the middle and upper atmosphere (MU) radar in midlatitudes (29.3 degrees N dip latitude). Utilizing the rapid beam-steering capability of the EAR, the spatial structure of the postmidnight irregularities is clearly presented for the first time. It is found that they usually propagate westward and can be categorized into two types. One shows sharp upwelling plumes near local midnight, which should not be a mere passage of fossil plasma bubbles. The other has successive tilted structures which have the same orientation as medium-scale traveling ionospheric disturbances typically observed at midlatitudes. We suggest that the convergence of the equatorward thermospheric wind which is believed to be responsible for the midnight temperature maximum may be an important factor to produce a preferable condition for the upwelling plumes in the postmidnight sector. The displacement between geographic and magnetic equators may also be important for seasonal/longitudinal variation of the postmidnight irregularities.
C1 [Yokoyama, T.; Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yokoyama, T.] Univ Maryland Baltimore Cty, Goddard Planetary & Heliophys Inst, Baltimore, MD 21228 USA.
[Yamamoto, M.] Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto 6110011, Japan.
[Otsuka, Y.; Nishioka, M.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Tsugawa, T.] Natl Inst Informat & Commun Technol, Tokyo 1848795, Japan.
[Watanabe, S.] Hokkaido Univ, Div Earth & Planetary Sci, Grad Sch Sci, Sapporo, Hokkaido 0600810, Japan.
RP Yokoyama, T (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 674, Greenbelt, MD 20771 USA.
EM tatsuhiro.yokoyama@nasa.gov
RI Watanabe, Shigeto/A-4305-2012; Pfaff, Robert/F-5703-2012
OI Pfaff, Robert/0000-0002-4881-9715
NR 55
TC 18
Z9 18
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 NOV 22
PY 2011
VL 116
AR A11325
DI 10.1029/2011JA016797
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853IW
UT WOS:000297420400001
ER
PT J
AU Yokoyama, T
Pfaff, RF
Roddy, PA
Yamamoto, M
Otsuka, Y
AF Yokoyama, T.
Pfaff, R. F.
Roddy, P. A.
Yamamoto, M.
Otsuka, Y.
TI On postmidnight low-latitude ionospheric irregularities during solar
minimum: 2. C/NOFS observations and comparisons with the Equatorial
Atmosphere Radar
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID REGION PLASMA DRIFTS; MIDLATITUDE IONOSPHERE; SPREAD-F; JICAMARCA
AB A detailed comparison between the observations of the Communication/Navigation Outage Forecasting System (C/NOFS) satellite and the 47 MHz Equatorial Atmosphere Radar (EAR) in West Sumatra, Indonesia (10.36 degrees S dip latitude) on the postmidnight irregularities is presented. The zonal and meridional E x B drift velocities measured by the vector electric field instrument on the C/NOFS are consistent with the westward propagation of backscatter echoes and the line-of-sight Doppler velocities observed with the EAR, respectively. The plasma density depletions are observed in the postmidnight sector for several consecutive orbits, which suggests the depletions grow slowly during the premidnight period and reach the spacecraft altitude around local midnight. The convergence of the equatorward wind which could be responsible for the midnight temperature maximum may produce a preferable condition for the growth of the Rayleigh-Taylor instability around midnight. Electric field fluctuations of medium-scale traveling ionospheric disturbances may play an important role in seeding the instability. Both equatorial and midlatitude-type plasma instabilities could be operational at the EAR latitude sector, which together would foster a high occurrence of postmidnight irregularities during solar minimum.
C1 [Yokoyama, T.; Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yokoyama, T.] Univ Maryland Baltimore Cty, Goddard Planetary & Heliophys Inst, Baltimore, MD 21228 USA.
[Roddy, P. A.] USAF, Space Vehicles Directorate, Res Lab, Bedford, MA 01731 USA.
[Yamamoto, M.] Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto 6110011, Japan.
[Otsuka, Y.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
RP Yokoyama, T (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 674, Greenbelt, MD 20771 USA.
EM tatsuhiro.yokoyama@nasa.gov
RI Pfaff, Robert/F-5703-2012
OI Pfaff, Robert/0000-0002-4881-9715
FU U.S. Air Force
FX The C/NOFS mission, conceived and developed by the Air Force Research
Laboratory, is sponsored and executed by the U.S. Air Force Space Test
Program. This research was carried out by the collaborative research
program of the Research Institute for Sustainable Humanosphere (RISH),
Kyoto University. The operation of EAR is based on the agreement between
RISH and LAPAN signed on 8 September 2000.
NR 24
TC 12
Z9 12
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD NOV 22
PY 2011
VL 116
AR A11326
DI 10.1029/2011JA016798
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853IW
UT WOS:000297420400002
ER
PT J
AU Chanan, G
Troy, M
Surdej, I
Gutt, G
Roberts, LC
AF Chanan, Gary
Troy, Mitchell
Surdej, Isabelle
Gutt, Gary
Roberts, Lewis C., Jr.
TI Fresnel phasing of segmented mirror telescopes
SO APPLIED OPTICS
LA English
DT Article
ID KECK TELESCOPES; TECHNOLOGIES; PERFORMANCE; ALGORITHM; SENSOR
AB Shack-Hartmann (S-H) phasing of segmented telescopes is based upon a physical optics generalization of the geometrical optics Shack-Hartmann test, in which each S-H lenslet straddles an intersegment edge. For the extremely large segmented telescopes currently in the design stages, one is led naturally to very large pupil demagnifications for the S-H phasing cameras. This in turn implies rather small Fresnel numbers F for the lenslets; the nominal design for the Thirty Meter Telescope calls for F = 0.6. For such small Fresnel numbers, it may be possible to eliminate the lenslets entirely, replacing them with a simple mask containing a sparse array of clear subapertures and thereby also eliminating a number of manufacturing problems and experimental complications associated with lenslets. We present laboratory results that demonstrate the validity of this approach. (C) 2011 Optical Society of America
C1 [Chanan, Gary] Univ Calif Irvine, Irvine, CA 92697 USA.
[Troy, Mitchell; Gutt, Gary; Roberts, Lewis C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Surdej, Isabelle] European Org Astron Res So Hemisphere ESO, D-85748 Garching, Germany.
RP Chanan, G (reprint author), Univ Calif Irvine, Irvine, CA 92697 USA.
EM gachanan@uci.edu
OI Roberts, Lewis/0000-0003-3892-2900
FU California Institute of Technology; National Aeronautics and Space
Administration (NASA); Gordon and Betty Moore Foundation; Canada
Foundation for Innovation; Ontario Ministry of Research and Innovation;
National Research Council of Canada (NRC); U.S. National Science
Foundation (NSF); TMT partner institutions
FX This research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, and was sponsored in part by the
California Institute of Technology and the National Aeronautics and
Space Administration (NASA). We also gratefully acknowledge the support
of the TMT partner institutions. They are the Association of Canadian
Universities for Research in Astronomy, the California Institute of
Technology, and the University of California. This work was supported as
well by the Gordon and Betty Moore Foundation, the Canada Foundation for
Innovation, the Ontario Ministry of Research and Innovation, the
National Research Council of Canada (NRC), and the U.S. National Science
Foundation (NSF).
NR 13
TC 2
Z9 2
U1 0
U2 4
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 NOV 20
PY 2011
VL 50
IS 33
BP 6283
EP 6293
DI 10.1364/AO.50.006283
PG 11
WC Optics
SC Optics
GA 852CL
UT WOS:000297324300020
PM 22108889
ER
PT J
AU Andersen, M
Rho, J
Reach, WT
Hewitt, JW
Bernard, JP
AF Andersen, M.
Rho, J.
Reach, W. T.
Hewitt, J. W.
Bernard, J. P.
TI DUST PROCESSING IN SUPERNOVA REMNANTS: SPITZER MIPS SPECTRAL ENERGY
DISTRIBUTION AND INFRARED SPECTROGRAPH OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: supernova remnants
ID AROMATIC-HYDROCARBON EMISSION; MHZ MASER EMISSION; X-RAY OBSERVATIONS;
INTERSTELLAR DUST; MOLECULAR CLOUDS; GALACTIC PLANE; SPACE-TELESCOPE;
DENSE CLOUDS; MILKY-WAY; J-SHOCKS
AB We present Spitzer Multiband Imaging Photometer (MIPS) spectral energy distribution (SED) and Infrared Spectrograph (IRS) observations of 14 Galactic supernova remnants (SNRs) previously identified in the GLIMPSE survey. We find evidence for SNR/molecular cloud interaction through detection of [OI] emission, ionic lines, and emission from molecular hydrogen. Through blackbody fitting of the MIPS SEDs we find the large grains to be warm, 29-66 K. The dust emission is modeled using the DUSTEM code and a three-component dust model composed of populations of big grains (BGs), very small grains (VSGs), and polycyclic aromatic hydrocarbons. We find the dust to be moderately heated, typically by 30-100 times the interstellar radiation field. The source of the radiation is likely hydrogen recombination, where the excitation of hydrogen occurred in the shock front. The ratio of VSGs to BGs is found for most of the molecular interacting SNRs to be higher than that found in the plane of the Milky Way, typically by a factor of 2-3. We suggest that dust shattering is responsible for the relative overabundance of small grains, in agreement with the prediction from dust destruction models. However, two of the SNRs are best fitted with a very low abundance of carbon grains to silicate grains and with a very high radiation field. A likely reason for the low abundance of small carbon grains is sputtering. We find evidence for silicate emission at 20 mu m in their SEDs, indicating that they are young SNRs based on the strong radiation field necessary to reproduce the observed SEDs.
C1 [Andersen, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Andersen, M.] European Space Agcy, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands.
[Rho, J.; Reach, W. T.] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hewitt, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bernard, J. P.] CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France.
RP Andersen, M (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
EM manderse@rssd.esa.int
OI Reach, William/0000-0001-8362-4094
FU Jet Propulsion Laboratory, California Institute of Technology, under
NASA [1407]; NASA; LTSA [NRA-01-01-LTSA-013]
FX We thank the anonymous referee for careful reading and insightful
comments which helped to improve the paper. 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. Partial support for this work was provided by both a
NASA Spitzer GO award issued by JPL/Caltech and an LTSA grant
NRA-01-01-LTSA-013. The DUSTEM code is available from
http://www.ias.u-psud.fr/DUSTEM/.
NR 65
TC 29
Z9 29
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
VL 742
IS 1
AR 7
DI 10.1088/0004-637X/742/1/7
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400007
ER
PT J
AU Cannizzo, JK
Troja, E
Lodato, G
AF Cannizzo, J. K.
Troja, E.
Lodato, G.
TI GRB 110328A/SWIFT J164449.3+573451: THE TIDAL OBLITERATION OF A DEEPLY
PLUNGING STAR?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: active;
galaxies: nuclei
ID MASSIVE BLACK-HOLE; GAMMA-RAY BURSTS; STELLAR DISRUPTION; ACCRETION
DISKS; NEARBY GALAXIES; GALACTIC NUCLEI; LIGHT CURVES; X-RAY; FLARES;
JETS
AB We examine the tidal disruption event (TDE) scenario to explain Sw 1644+57, a powerful and persistent X-ray source which suddenly became active as GRB 110328A. The precise localization at the center of a z = 0.35 galaxy argues for activity of the central engine as the underlying cause. We look at the suggestion by Bloom et al. of the possibility of a TDE. We argue that Sw 1644+57 cannot be explained by the traditional TDE model in which the periastron distance is close to the tidal disruption radius-three independent lines of argument indicate the orbit must be deeply plunging or else the powerful jet we are observing could not be produced. These arguments stem from (1) comparing the early X-ray light curve to the expected theoretical fallback rate, (2) looking at the time of transition to disk-dominated decay, and (3) considering the TDE rate. Due to the extreme excess in the tidal force above that which would be required minimally to disrupt the star in a deeply plunging orbit at periastron, we suggest this scenario might be referred to more descriptively as a tidal obliteration event (TOE) rather than a TDE.
C1 [Cannizzo, J. K.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
[Cannizzo, J. K.; Troja, E.] NASA GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Cannizzo, J. K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Lodato, G.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy.
RP Cannizzo, JK (reprint author), NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
EM John.K.Cannizzo@nasa.gov
FU Goddard Space Flight Center; NASA
FX We thank L. Piro and E. Rossi for useful conversations. This work made
use of data supplied by the UK Swift Science Data Centre at the
University of Leicester. E. T. was supported by an appointment to the
NASA Postdoctoral Program at the Goddard Space Flight Center,
administered by the Oak Ridge Associated Universities through a contract
with NASA.
NR 54
TC 30
Z9 30
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 NOV 20
PY 2011
VL 742
IS 1
AR 32
DI 10.1088/0004-637X/742/1/32
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400032
ER
PT J
AU Darling, J
Macdonald, EP
Haynes, MP
Giovanelli, R
AF Darling, Jeremy
Macdonald, Erin P.
Haynes, Martha P.
Giovanelli, Riccardo
TI THE ALFALFA Hi ABSORPTION PILOT SURVEY: A WIDE-AREA BLIND DAMPED Ly
alpha SYSTEM SURVEY OF THE LOCAL UNIVERSE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: observational; quasars: absorption lines; radio lines:
galaxies; surveys
ID SKY SURVEY; RADIO-SOURCES; CATALOG; IV
AB We present the results of a pilot survey for neutral hydrogen (H i) 21 cm absorption in the Arecibo Legacy Fast Arecibo L-Band Feed Array (ALFALFA) Survey. This project is a wide-area "blind" search for Hi absorption in the local universe, spanning -650 km s(-1) < cz < 17,500 km s(-1) and covering 517.0 deg(2) (7% of the full ALFALFA survey). The survey is sensitive to Hi absorption lines stronger than 7.7 mJy (8983 radio sources) and is 90% complete for lines stronger than 11.0 mJy (7296 sources). The total redshift interval sensitive to all damped Ly alpha (DLA) systems (N(Hi) >= 2 x 10(20) cm(-2)) is Delta z = 7.0 (129 objects, assuming T(s) = 100 K and covering fraction unity); for super-DLAs (N(Hi) >= 2 x 10(21) cm(-2)) it is Delta z = 128.2 (2353 objects). We re-detect the intrinsic Hi absorption line in UGC 6081 but detect no intervening absorption line systems. We compute a 95% confidence upper limit on the column density frequency distribution function f (NHi, X) spanning four orders of magnitude in column density, 10(19) (T(s)/100 K) (1/f) cm(-2) < N(Hi) < 10(23) (T(s)/100 K) (1/f) cm(-2), that is consistent with previous redshifted optical DLA surveys and the aggregate Hi 21 cm emission in the local universe. The detection rate is in agreement with extant observations. This pilot survey suggests that an absorption line search of the complete ALFALFA survey-or any higher redshift, larger bandwidth, or more sensitive survey, such as those planned for Square Kilometer Array pathfinders or a low-frequency lunar array-will either make numerous detections or will set a strong statistical lower limit on the typical spin temperature of neutral hydrogen gas.
C1 [Darling, Jeremy; Macdonald, Erin P.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Darling, Jeremy] NASA Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA USA.
[Macdonald, Erin P.] Univ Glasgow, Sch Phys & Astron, Inst Gravitat Res, Glasgow G12 8QQ, Lanark, Scotland.
[Haynes, Martha P.; Giovanelli, Riccardo] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Haynes, Martha P.; Giovanelli, Riccardo] Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA.
RP Darling, J (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, 389 UCB, Boulder, CO 80309 USA.
EM jdarling@colorado.edu; e.macdonald@physics.gla.ac.uk;
haynes@astro.cornell.edu; riccardo@astro.cornell.edu
RI Darling, Jeremy/A-7968-2009
OI Darling, Jeremy/0000-0003-2511-2060
FU NSF [AST-0607007]; Brinson Foundation; NASA Lunar Science Institute,
NASA Lunar Science Institute [NNA09DB30A]; National Aeronautics and
Space Administration; National Science Foundation; Alfred P. Sloan
Foundation; Participating Institutions, the National Science Foundation;
U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society;
Higher Education Funding Council for England
FX The authors thank the members of the ALFALFA team who have contributed
to the acquisition and processing of the ALFALFA data set, especially
Amelie Saintonge and Brian Kent for the software they developed for
general implementation within the ALFALFA data processing software
package. The authors thank Jason X. Prochaska for critical questions and
help with the calculation of the column density frequency distribution
function. We also thank the anonymous referees for extremely helpful
feedback. R. G. and M. P. H. are supported by NSF grant AST-0607007 and
by a grant from the Brinson Foundation. The LUNAR consortium
(http://lunar.colorado.edu), headquartered at the University of
Colorado, is funded by the NASA Lunar Science Institute (via Cooperative
Agreement NNA09DB30A) to investigate concepts for astrophysical
observatories on the Moon. This 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. 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. Funding for the SDSS
and SDSS-II has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, the U.S.
Department of Energy, the National Aeronautics and Space Administration,
the Japanese Monbukagakusho, the Max Planck Society, and the Higher
Education Funding Council for England. The SDSS Web site is
http://www.sdss.org/.
NR 19
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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 NOV 20
PY 2011
VL 742
IS 1
AR 60
DI 10.1088/0004-637X/742/1/60
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400060
ER
PT J
AU Grav, T
Mainzer, AK
Bauer, J
Masiero, J
Spahr, T
McMillan, RS
Walker, R
Cutri, R
Wright, E
Eisenhardt, PRM
Blauvelt, E
DeBaun, E
Elsbury, D
Gautier, T
Gomillion, S
Hand, E
Wilkins, A
AF Grav, T.
Mainzer, A. K.
Bauer, J.
Masiero, J.
Spahr, T.
McMillan, R. S.
Walker, R.
Cutri, R.
Wright, E.
Eisenhardt, P. R. M.
Blauvelt, E.
DeBaun, E.
Elsbury, D.
Gautier, T.
Gomillion, S.
Hand, E.
Wilkins, A.
TI WISE/NEOWISE OBSERVATIONS OF THE JOVIAN TROJANS: PRELIMINARY RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; minor planets, asteroids: general; surveys
ID INFRARED-SURVEY-EXPLORER; NEAR-EARTH ASTEROIDS; SOLAR-SYSTEM;
SPECTROSCOPIC SURVEY; SIZE DISTRIBUTION; THERMAL-MODEL; JUPITER; ORIGIN;
POPULATION; PHOTOMETRY
AB We present the preliminary analysis of over 1739 known and 349 candidate Jovian Trojans observed by the NEOWISE component of the Wide-field Infrared Survey Explorer (WISE). With this survey the available diameters, albedos, and beaming parameters for the Jovian Trojans have been increased by more than an order of magnitude compared to previous surveys. We find that the Jovian Trojan population is very homogenous for sizes larger than similar to 10 km (close to the detection limit of WISE for these objects). The observed sample consists almost exclusively of low albedo objects, having a mean albedo value of 0.07 +/- 0.03. The beaming parameter was also derived for a large fraction of the observed sample, and it is also very homogenous with an observed mean value of 0.88 +/- 0.13. Preliminary debiasing of the survey shows that our observed sample is consistent with the leading cloud containing more objects than the trailing cloud. We estimate the fraction to be N(leading)/N(trailing) similar to 1.4 +/- 0.2, lower than the 1.6 +/- 0.1 value derived by Szabo et al.
C1 [Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Mainzer, A. K.; Bauer, J.; Masiero, J.; Eisenhardt, P. R. M.; Blauvelt, E.; DeBaun, E.; Elsbury, D.; Gautier, T.; Gomillion, S.; Hand, E.; Wilkins, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J.; Cutri, R.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Walker, R.] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Wright, E.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA.
[Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Grav, T (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM tgrav@pha.jhu.edu
OI Blauvelt, Erin/0000-0002-2944-5818; Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This publication also makes use of data products from
NEOWISE, which is a project of the Jet Propulsion Laboratory/California
Institute of Technology, funded by the Planetary Science Division of the
National Aeronautics and Space Administration. We gratefully acknowledge
the extraordinary services specific to NEOWISE contributed by the
International Astronomical 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 also thank
the worldwide community of dedicated amateur and professional
astronomers devoted to minor planet follow-up observations. This
research has made use the NASA/IPAC Infrared Science Archive, which is
operated by the Jet Propulsion Laboratory/California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 48
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U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
VL 742
IS 1
AR 40
DI 10.1088/0004-637X/742/1/40
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400040
ER
PT J
AU Lapi, A
Gonzalez-Nuevo, J
Fan, L
Bressan, A
De Zotti, G
Danese, L
Negrello, M
Dunne, L
Eales, S
Maddox, S
Auld, R
Baes, M
Bonfield, DG
Buttiglione, S
Cava, A
Clements, DL
Cooray, A
Dariush, A
Dye, S
Fritz, J
Herranz, D
Hopwood, R
Ibar, E
Ivison, R
Jarvis, MJ
Kaviraj, S
Lopez-Caniego, M
Massardi, M
Michallowski, MJ
Pascale, E
Pohlen, M
Rigby, E
Rodighiero, G
Serjeant, S
Smith, DJB
Temi, P
Wardlow, J
van der Werf, P
AF Lapi, A.
Gonzalez-Nuevo, J.
Fan, L.
Bressan, A.
De Zotti, G.
Danese, L.
Negrello, M.
Dunne, L.
Eales, S.
Maddox, S.
Auld, R.
Baes, M.
Bonfield, D. G.
Buttiglione, S.
Cava, A.
Clements, D. L.
Cooray, A.
Dariush, A.
Dye, S.
Fritz, J.
Herranz, D.
Hopwood, R.
Ibar, E.
Ivison, R.
Jarvis, M. J.
Kaviraj, S.
Lopez-Caniego, M.
Massardi, M.
Michallowski, M. J.
Pascale, E.
Pohlen, M.
Rigby, E.
Rodighiero, G.
Serjeant, S.
Smith, D. J. B.
Temi, P.
Wardlow, J.
van der Werf, P.
TI HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE
FORMATION OF MASSIVE EARLY-TYPE GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift;
submillimeter: galaxies
ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE
BLACK-HOLES; SCIENCE DEMONSTRATION PHASE; DARK-MATTER HALOES; 250 MU-M;
SUBMILLIMETER NUMBER COUNTS; FAR-INFRARED PROPERTIES; STAR-FORMATION
HISTORY; LARGE-SCALE STRUCTURE
AB Exploiting the Herschel Astrophysical Terahertz Large Area Survey Science Demonstration Phase survey data, we have determined the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 mu m and at several redshifts z greater than or similar to 1, for bright submillimeter galaxies with star formation rates (SFRs) greater than or similar to 100 M-circle dot yr(-1). We find that the evolution of the comoving LF is strong up to z approximate to 2.5, and slows down at higher redshifts. From the LFs and the information on halo masses inferred from clustering analysis, we derived an average relation between SFR and halo mass (and its scatter). We also infer that the timescale of the main episode of dust-enshrouded star formation in massive halos (M-H greater than or similar to 3 x 10(12) M-circle dot) amounts to similar to 7 x 10(8) yr. Given the SFRs, which are in the range of 10(2)-10(3) M-circle dot yr(-1), this timescale implies final stellar masses of the order of 10(11)-10(12) M-circle dot. The corresponding stellar mass function matches the observed mass function of passively evolving galaxies at z greater than or similar to 1. The comparison of the statistics for submillimeter and UV-selected galaxies suggests that the dust-free, UV bright phase is greater than or similar to 10(2) times shorter than the submillimeter bright phase, implying that the dust must form soon after the onset of star formation. Using a single reference spectral energy distribution (SED; the one of the z approximate to 2.3 galaxy SMM J2135-0102), our simple physical model is able to reproduce not only the LFs at different redshifts >1 but also the counts at wavelengths ranging from 250 mu m to approximate to 1 mm. Owing to the steepness of the counts and their relatively broad frequency range, this result suggests that the dispersion of submillimeter SEDs of z > 1 galaxies around the reference one is rather small.
C1 [Lapi, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Lapi, A.; Gonzalez-Nuevo, J.; Fan, L.; Bressan, A.; De Zotti, G.; Danese, L.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Fan, L.] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China.
[Bressan, A.; De Zotti, G.; Buttiglione, S.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Negrello, M.; Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Dunne, L.; Maddox, S.; Rigby, E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Eales, S.; Auld, R.; Dariush, A.; Dye, S.; Kaviraj, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Bonfield, D. G.; Jarvis, M. J.; Smith, D. J. B.] Univ Hertfordshire, Ctr Astrophys, Hatfield AL10 9AB, Herts, England.
[Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain.
[Clements, D. L.; Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Herranz, D.; Lopez-Caniego, M.] Inst Fis Cantabria CSIC UC, Santander 39005, Spain.
[Ibar, E.; Ivison, R.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R.; Michallowski, M. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
[Massardi, M.] INAF IRA, I-40129 Bologna, Italy.
[Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[van der Werf, P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
RP Lapi, A (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy.
RI Baes, Maarten/I-6985-2013; Lopez-Caniego, Marcos/M-4695-2013; Herranz,
Diego/K-9143-2014; Wardlow, Julie/C-9903-2015; Gonzalez-Nuevo,
Joaquin/I-3562-2014; Ivison, R./G-4450-2011; Fan, Lulu/P-2168-2016;
Cava, Antonio/C-5274-2017;
OI Dye, Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X;
Rodighiero, Giulia/0000-0002-9415-2296; Baes,
Maarten/0000-0002-3930-2757; Herranz, Diego/0000-0003-4540-1417;
Wardlow, Julie/0000-0003-2376-8971; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; Ivison, R./0000-0001-5118-1313; Fan,
Lulu/0000-0003-4200-4432; Cava, Antonio/0000-0002-4821-1275;
Lopez-Caniego, Marcos/0000-0003-1016-9283; Maddox,
Stephen/0000-0001-5549-195X
FU ASI/INAF [I/009/10/0]; INAF
FX The work has been supported in part by ASI/INAF agreement No. I/009/10/0
and by INAF through the PRIN 2009 "New light on the early Universe with
sub-mm spectroscopy." We thank the referee for helpful comments and
suggestions, and Cedric Lacey who provided in tabular form the
submillimeter counts yielded by the Lacey et al. (2010) model. A. Lapi
acknowledges useful discussions with A. Cavaliere, G. L. Granato, P.
Salucci, L. Silva, and F. Shankar, and thanks SISSA and INAF-OATS for
warm hospitality.
NR 148
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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 NOV 20
PY 2011
VL 742
IS 1
AR 24
DI 10.1088/0004-637X/742/1/24
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400024
ER
PT J
AU Lister, ML
Aller, M
Aller, H
Hovatta, T
Kellermann, KI
Kovalev, YY
Meyer, ET
Pushkarev, AB
Ros, E
Ackermann, M
Antolini, E
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Boeck, M
Bonamente, E
Borgland, AW
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cavazzuti, E
Cecchi, C
Chang, CS
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
de Palma, F
Dermer, CD
Silva, EDE
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Fegan, SJ
Ferrara, EC
Finke, J
Focke, WB
Fortin, P
Fukazawa, Y
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
Horan, D
Hughes, RE
Johannesson, G
Johnson, AS
Kadler, M
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Mazziotta, MN
McConville, W
McEnery, JE
Mehault, J
Michelson, PF
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nishino, S
Nolan, PL
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ozaki, M
Paneque, D
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Raino, S
Readhead, A
Reimer, A
Reimer, O
Richards, JL
Ritz, S
Sadrozinski, HFW
Sgro, C
Shaw, MS
Siskind, EJ
Spandre, G
Spinelli, P
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tosti, G
Tramacere, A
Troja, E
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Wang, P
Winer, BL
Wood, KS
Zimmer, S
AF Lister, M. L.
Aller, M.
Aller, H.
Hovatta, T.
Kellermann, K. I.
Kovalev, Y. Y.
Meyer, E. T.
Pushkarev, A. B.
Ros, E.
Ackermann, M.
Antolini, E.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Boeck, M.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Chang, C. S.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Finke, J.
Focke, W. B.
Fortin, P.
Fukazawa, Y.
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.
Horan, D.
Hughes, R. E.
Johannesson, G.
Johnson, A. S.
Kadler, M.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Mazziotta, M. N.
McConville, W.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Naumann-Godo, M.
Nishino, S.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ozaki, M.
Paneque, D.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Raino, S.
Readhead, A.
Reimer, A.
Reimer, O.
Richards, J. L.
Ritz, S.
Sadrozinski, H. F-W
Sgro, C.
Shaw, M. S.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tosti, G.
Tramacere, A.
Troja, E.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Zimmer, S.
CA Collaboration, M
FERMI LAT Collaboration
TI gamma-RAY AND PARSEC-SCALE JET PROPERTIES OF A COMPLETE SAMPLE OF
BLAZARS FROM THE MOJAVE PROGRAM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; galaxies: active; galaxies: jets; gamma
rays: galaxies; quasars: general; radio continuum: galaxies
ID ACTIVE GALACTIC NUCLEI; BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE;
EXTRAGALACTIC RADIO-SOURCES; DIGITAL SKY SURVEY; READHEAD SURVEY
SOURCES; QUASI-STELLAR OBJECTS; BANK 966-MHZ SURVEY; BASE-LINE ARRAY;
OPTICAL SPECTROSCOPY
AB We investigate the Fermi Large Area Telescope gamma-ray and 15 GHz Very Long Baseline Array radio properties of a joint gamma-ay and radio-selected sample of active galactic nuclei (AGNs) obtained during the first 11 months of the Fermi mission (2008 August 4-2009 July 5). Our sample contains the brightest 173 AGNs in these bands above declination -30 degrees during this period, and thus probes the full range of gamma-ray loudness (gamma-ray to radio band luminosity ratio) in the bright blazar population. The latter quantity spans at least 4 orders of magnitude, reflecting a wide range of spectral energy distribution (SED) parameters in the bright blazar population. The BL Lac objects, however, display a linear correlation of increasing gamma-ray loudness with synchrotron SED peak frequency, suggesting a universal SED shape for objects of this class. The synchrotron self-Compton model is favored for the gamma-ray emission in these BL Lac objects over external seed photon models, since the latter predict a dependence of Compton dominance on Doppler factor that would destroy any observed synchrotron SED-peak-gamma-ray-loudness correlation. The high-synchrotron peaked (HSP) BL Lac objects are distinguished by lower than average radio core brightness temperatures, and none display large radio modulation indices or high linear core polarization levels. No equivalent trends are seen for the flat-spectrum radio quasars (FSRQs) in our sample. Given the association of such properties with relativistic beaming, we suggest that the HSP BL Lac objects have generally lower Doppler factors than the lower-synchrotron peaked BL Lac objects or FSRQs in our sample.
C1 [Lister, M. L.; Hovatta, T.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Aller, M.; Aller, H.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Hovatta, T.] Owens Valley Radio Observ, Big Pine, CA 93513 USA.
[Kellermann, K. I.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia.
[Kovalev, Y. Y.; Pushkarev, A. B.; Ros, E.; Chang, C. S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Meyer, E. T.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia.
[Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine.
[Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Ackermann, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Shaw, M. S.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ackermann, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Shaw, M. S.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, 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.; Pierbattista, M.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,Serv Astrophys,CEA Saclay, 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.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Boeck, M.; Kadler, M.] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany.
[Boeck, M.; Kadler, M.] ECAP, D-96049 Bamberg, Germany.
[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.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Chang, C. S.] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France.
[Conrad, J.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Dermer, C. D.; Finke, J.; Lovellette, M. N.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Ferrara, E. C.; Gehrels, N.; Hays, E.; Kadler, M.; McConville, W.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Mizuno, T.; Nishino, S.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Kadler, M.] CRESST, Greenbelt, MD 20771 USA.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France.
[Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etudes Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[McConville, W.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McConville, W.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohno, M.; Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Readhead, A.; Richards, J. L.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 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.
[Ritz, S.; Sadrozinski, H. F-W] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Ritz, S.; Sadrozinski, H. F-W] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Lister, ML (reprint author), Purdue Univ, Dept Phys, 525 Northwestern Ave, W Lafayette, IN 47907 USA.
EM mlister@purdue.edu; moritz.boeck@sternwarte.uni-erlangen.de
RI Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Pushkarev,
Alexander/M-9997-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Orlando, E/R-5594-2016; Hays,
Elizabeth/D-3257-2012; Thompson, David/D-2939-2012; Kovalev,
Yuri/J-5671-2013; Johannesson, Gudlaugur/O-8741-2015; 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
OI Loparco, Francesco/0000-0002-1173-5673; Gargano,
Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672; SPINELLI,
Paolo/0000-0001-6688-8864; Thompson, David/0000-0001-5217-9135; Kovalev,
Yuri/0000-0001-9303-3263; Johannesson, Gudlaugur/0000-0003-1458-7036;
lubrano, pasquale/0000-0003-0221-4806; giglietto,
nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Reimer,
Olaf/0000-0001-6953-1385;
FU K. A. Wallenberg Foundation; EU [MEST-CT-2005-19669]; Alexander von
Humboldt Foundation; Russian Foundation for Basic Research (RFBR)
[08-02-00545, 11-02-00368]; Spanish MICINN [AYA2009-13036-C02-02]; NSF;
NASA; University of Michigan; National Science Foundation [AST-0807860];
NASA [NNX08AV67G]
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; C. S. Chang was a former member
of the International Max Planck Research School for Astronomy and
Astrophysics. C. S. Chang acknowledges support by the EU Framework 6
Marie Curie Early Stage Training programme under contract number
MEST-CT-2005-19669 "Estrela."; Y. Y. Kovalev was supported in part by
the return fellowship of the Alexander von Humboldt Foundation and the
Russian Foundation for Basic Research (RFBR) grants 08-02-00545 and
11-02-00368.; E. Ros acknowledges partial support by the Spanish MICINN
through grant AYA2009-13036-C02-02.; Work at UMRAO was made possible by
grants from the NSF and NASA and by support from the University of
Michigan. The Fermi LAT Collaboration acknowledges generous ongoing
support from a number of agencies and institutes that have supported
both the development and the operation of the LAT as well as scientific
data analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'EnergieAtomique and the Centre National de la Recherche
Scientifique/Institut National de Physique Nucleaire et de Physique des
Particules in France, the Agenzia Spaziale Italiana and the Istituto
Nazionale di Fisica Nucleare in Italy, the Ministry of Education,
Culture, Sports, Science and Technology (MEXT), High Energy Accelerator
Research Organization (KEK) and Japan Aerospace Exploration Agency
(JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.; The
MOJAVE project is supported under National Science Foundation grant
AST-0807860 and NASA Fermi grant NNX08AV67G.
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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 NOV 20
PY 2011
VL 742
IS 1
AR 27
DI 10.1088/0004-637X/742/1/27
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400027
ER
PT J
AU Olausen, SA
Kaspi, VM
Ng, CY
Zhu, WW
Dib, R
Gavriil, FP
Woods, PM
AF Olausen, S. A.
Kaspi, V. M.
Ng, C. -Y.
Zhu, W. W.
Dib, R.
Gavriil, F. P.
Woods, P. M.
TI ON THE EXTENDED EMISSION AROUND THE ANOMALOUS X-RAY PULSAR 1E
1547.0-5408
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (1E 1547.0-5408); stars: neutron; X-rays: stars
ID SOFT GAMMA-REPEATERS; MAGNETIZED NEUTRON-STARS; PHOTON IMAGING CAMERA;
27 GIANT FLARE; SGR 1806-20; SUPERNOVA REMNANT; INTERSTELLAR GRAINS;
2009 OUTBURST; XMM-NEWTON; SPIN-DOWN
AB We present an analysis of the extended emission around the anomalous X-ray pulsar 1E 1547.0-5408 using four XMM-Newton observations taken with the source in varying states of outburst as well as in quiescence. We find that the extended emission flux is highly variable and strongly correlated with the flux of the magnetar. Based on this result, as well as on spectral and energetic considerations, we conclude that the extended emission is dominated by a dust-scattering halo and not a pulsar wind nebula (PWN), as has been previously argued. We obtain an upper limit on the 2-10 keV flux of a possible PWN of 4.7 x 10(-14) erg s(-1) cm(-2), three times less than the previously claimed value, implying an efficiency for conversion of spin-down energy into nebular luminosity of <9 x 10(-4) (assuming a distance of 4 kpc). We do, however, find strong evidence for X-ray emission from the supernova remnant shell surrounding the pulsar, as previously reported.
C1 [Olausen, S. A.; Kaspi, V. M.; Ng, C. -Y.; Zhu, W. W.; Dib, R.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[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.] Dynetics Inc, Huntsville, AL 35806 USA.
[Woods, P. M.] Corvid Technol, Huntsville, AL 35806 USA.
RP Olausen, SA (reprint author), McGill Univ, Dept Phys, Rutherford Phys Bldg,3600 Univ St, Montreal, PQ H3A 2T8, Canada.
RI Ng, Chi Yung/A-7639-2013
OI Ng, Chi Yung/0000-0002-5847-2612
FU ESA Member States; NASA; NSERC; FQRNT via the Centre de Recherche
Astrophysique du Quebec; CIFAR; Killam Research Fellowship
FX This research is based on observations obtained with XMM-Newton, an ESA
science mission with instruments and contributions directly funded by
ESA Member States and NASA. V.M.K. receives support from NSERC via a
Discovery Grant, FQRNT via the Centre de Recherche Astrophysique du
Quebec, CIFAR, a Killam Research Fellowship, and holds a Canada Research
Chair and the Lorne Trottier Chair in Astrophysics and Cosmology.
C.-Y.N. is a CRAQ postdoctoral fellow and a Tomlinson postdoctoral
fellow.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
VL 742
IS 1
AR 4
DI 10.1088/0004-637X/742/1/4
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400004
ER
PT J
AU Rafferty, DA
Brandt, WN
Alexander, DM
Xue, YQ
Bauer, FE
Lehmer, BD
Luo, B
Papovich, C
AF Rafferty, D. A.
Brandt, W. N.
Alexander, D. M.
Xue, Y. Q.
Bauer, F. E.
Lehmer, B. D.
Luo, B.
Papovich, C.
TI SUPERMASSIVE BLACK HOLE GROWTH IN STARBURST GALAXIES OVER COSMIC TIME:
CONSTRAINTS FROM THE DEEPEST CHANDRA FIELDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: starburst; infrared: galaxies; stars:
formation
ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; EXTENDED GROTH
STRIP; STAR-FORMATION RATE; X-RAY SOURCES; SPECTRAL
ENERGY-DISTRIBUTIONS; GOODS-SOUTH FIELD; YALE-CHILE MUSYC; SPITZER
MIDINFRARED SPECTROSCOPY; PALOMAR-GREEN QUASARS
AB We present an analysis of deep multiwavelength data for z approximate to 0.3-3 starburst galaxies selected by their 70 mu m emission in the Extended-Chandra Deep Field-South and Extended Groth Strip. We identify active galactic nuclei (AGNs) in these infrared sources through their X-ray emission and quantify the fraction that host an AGN. We find that the fraction depends strongly on both the mid-infrared color and rest-frame mid-infrared luminosity of the source, rising to similar to 50%-70% at the warmest colors (F-24 (mu m)/F-70 (mu m) less than or similar to 0.2) and highest mid-infrared luminosities (corresponding to ultraluminous infrared galaxies), similar to the trends found locally. Additionally, we find that the AGN fraction depends strongly on the star formation rate (SFR) of the host galaxy (inferred from the observed-frame 70 mu m luminosity after subtracting the estimated AGN contribution), particularly for more luminous AGNs (L0.5-8.0keV greater than or similar to 10(43) erg s(-1)). At the highest SFRs (similar to 1000 M-circle dot yr(-1)), the fraction of galaxies with an X-ray detected AGN rises to approximate to 30%, roughly consistent with that found in high-redshift submillimeter galaxies. Assuming that the AGN fraction is driven by the SFR (rather than stellar mass or redshift, for which our sample is largely degenerate), this result implies that the duty cycle of luminous AGN activity increases with the SFR of the host galaxy: specifically, we find that luminous X-ray detected AGNs are at least similar to 5-10 times more common in systems with high SFRs (greater than or similar to 300 M-circle dot yr(-1)) than in systems with lower SFRs (less than or similar to 30 M-circle dot yr(-1)). Lastly, we investigate the ratio between the supermassive black hole accretion rate (inferred from the AGN X-ray luminosity) and the bulge growth rate of the host galaxy (approximated as the SFR) and find that, for sources with detected AGNs and star formation (and neglecting systems with low star formation rates to which our data are insensitive), this ratio in distant starbursts agrees well with that expected from the local scaling relation assuming the black holes and bulges grew at the same epoch. These results imply that black holes and bulges grow together during periods of vigorous star formation and AGN activity.
C1 [Rafferty, D. A.; Brandt, W. N.; Xue, Y. Q.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Rafferty, D. A.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Alexander, D. M.; Lehmer, B. D.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 22, Chile.
[Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Papovich, C.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
RP Rafferty, DA (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
RI Brandt, William/N-2844-2015;
OI Brandt, William/0000-0002-0167-2453; Alexander,
David/0000-0002-5896-6313
FU NASA [SP8-9003A, NNX10AC99G]; Chandra X-ray Observatory Center
[SPO8-9003B]; Royal Society; Philip Leverhulme Prize
FX Support for this work was provided by NASA through Chandra Awards
SP8-9003A (D.A.R., W.N.B., Y.X., and B.L.) and SPO8-9003B (F.E.B.)
issued by the Chandra X-ray Observatory Center, which is operated by the
Smithsonian Astrophysical Observatory. We also acknowledge NASA ADP
grant NNX10AC99G (D.A.R., W.N.B., and Y.X.), the Royal Society (D.M.A.),
and a Philip Leverhulme Prize (D.M.A.) for support. We also thank M.
Dickinson for helpful feedback and A. Goulding and J. Mullaney for help
in interpreting the AGN SEDs and mid-infrared color ratios, and we thank
the referee for insightful comments that greatly improved the paper.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
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IS 1
AR 3
DI 10.1088/0004-637X/742/1/3
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400003
ER
PT J
AU Tombesi, F
Cappi, M
Reeves, JN
Palumbo, GGC
Braito, V
Dadina, M
AF Tombesi, F.
Cappi, M.
Reeves, J. N.
Palumbo, G. G. C.
Braito, V.
Dadina, M.
TI EVIDENCE FOR ULTRA-FAST OUTFLOWS IN RADIO-QUIET ACTIVE GALACTIC NUCLEI.
II. DETAILED PHOTOIONIZATION MODELING OF Fe K-SHELL ABSORPTION LINES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: active; galaxies: Seyfert; line:
identification; plasmas; X-rays: galaxies
ID X-RAY-SPECTRUM; ACCRETION DISC OUTFLOWS; XMM-NEWTON; BLACK-HOLE; GRATING
SPECTROMETER; SEYFERT-GALAXIES; IRON LINE; EMISSION; QUASAR; GAS
AB X-ray absorption line spectroscopy has recently shown evidence for previously unknown Ultra-fast Outflows (UFOs) in radio-quiet active galactic nuclei (AGNs). These have been detected essentially through blueshifted Fe xxv/xxvi K-shell transitions. In the previous paper of this series we defined UFOs as those highly ionized absorbers with an outflow velocity higher than 10,000 km s(-1) and assessed the statistical significance of the associated blueshifted absorption lines in a large sample of 42 local radio-quiet AGNs observed with XMM-Newton. The present paper is an extension of that work. First, we report a detailed curve of growth analysis of the main Fe xxv/xxvi transitions in photoionized plasmas. Then, we estimate an average spectral energy distribution for the sample sources and directly model the Fe K absorbers in the XMM-Newton spectra with the detailed Xstar photoionization code. We confirm that the frequency of sources in the radio-quiet sample showing UFOs is >35% and that the majority of the Fe K absorbers are indeed associated with UFOs. The outflow velocity distribution spans from similar to 10,000 km s(-1) (similar to 0.03c) up to similar to 100,000 km s(-1) (similar to 0.3c), with a peak and mean value of similar to 42,000 km s(-1) (similar to 0.14c). The ionization parameter is very high and in the range log xi similar to 3-6 erg s(-1) cm, with a mean value of log xi similar to 4.2 erg s(-1) cm. The associated column densities are also large, in the range N-H similar to 10(22)-10(24) cm(-2), with a mean value of N-H similar to 10(23) cm(-2). We discuss and estimate how selection effects, such as those related to the limited instrumental sensitivity at energies above 7 keV, may hamper the detection of even higher velocities and higher ionization absorbers. We argue that, overall, these results point to the presence of extremely ionized and possibly almost Compton-thick outflowing material in the innermost regions of AGNs. This also suggests that UFOs may potentially play a significant role in the expected cosmological feedback from AGNs and their study can provide important clues on the connection between accretion disks, winds, and jets.
C1 [Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Tombesi, F.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Tombesi, F.; Palumbo, G. G. C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Tombesi, F.; Cappi, M.; Dadina, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Reeves, J. N.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Tombesi, F (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
EM ftombesi@astro.umd.edu
RI Cappi, Massimo/F-4813-2015;
OI Cappi, Massimo/0000-0001-6966-8920; Dadina, Mauro/0000-0002-7858-7564;
Braito, Valentina/0000-0002-2629-4989
FU NASA; National Aeronautics and Space Administration; ASI [INAF/ASI
I/088/06/0]; UK STFC research council
FX F. T. thanks T. R. Kallman for the useful discussions on the use of the
Xstar code. F. T. thanks T. Yaqoob and the Johns Hopkins University for
the visiting period spent there doing part of this work. F. T. thanks C.
S. Reynolds for useful discussions. This paper is based on observations
obtained with the XMM-Newton satellite, an ESA funded mission with
contributions by the ESA member states and the USA. F. T. acknowledges
support from NASA through the ADAP/LTSA program. 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. M. C.,
G. G. C. P., and M. D. acknowledge support from ASI under the contract
INAF/ASI I/088/06/0. V. B. acknowledges support from the UK STFC
research council. The authors thank the anonymous referee for
suggestions that led to important improvements in the paper.
NR 56
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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 NOV 20
PY 2011
VL 742
IS 1
AR 44
DI 10.1088/0004-637X/742/1/44
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400044
ER
PT J
AU Whittet, DCB
Cook, AM
Herbst, E
Chiar, JE
Shenoy, SS
AF Whittet, D. C. B.
Cook, A. M.
Herbst, Eric
Chiar, J. E.
Shenoy, S. S.
TI OBSERVATIONAL CONSTRAINTS ON METHANOL PRODUCTION IN INTERSTELLAR AND
PREPLANETARY ICES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; dust, extinction; evolution; ISM: clouds; ISM:
molecules; stars: pre-main sequence
ID SPITZER SPECTROSCOPIC SURVEY; YOUNG STELLAR OBJECTS; TAURUS DARK CLOUDS;
LOW-MASS STARS; INFRARED BAND STRENGTHS; SOLID CARBON-DIOXIDE; GAS-GRAIN
CHEMISTRY; MOLECULAR CLOUDS; CO2 ICE; LABORATORY SIMULATIONS
AB Methanol (CH3OH) is thought to be an important link in the chain of chemical evolution that leads from simple diatomic interstellar molecules to complex organic species in protoplanetary disks that may be delivered to the surfaces of Earthlike planets. Previous research has shown that CH3OH forms in the interstellar medium predominantly on the surfaces of dust grains. To enhance our understanding of the conditions that lead to its efficient production, we assemble a homogenized catalog of published detections and limiting values in interstellar and preplanetary ices for both CH3OH and the other commonly observed C-and O-bearing species, H2O, CO, and CO2. We use this catalog to investigate the abundance of ice-phase CH3OH in environments ranging from dense molecular clouds to circumstellar envelopes around newly born stars of low and high mass. Results show that CH3OH production arises during the CO freezeout phase of ice-mantle growth in the clouds, after an ice layer rich in H2O and CO2 is already in place on the dust, in agreement with current astrochemical models. The abundance of solid-phase CH3OH in this environment is sufficient to account for observed gas-phase abundances when the ices are subsequently desorbed in the vicinity of embedded stars. CH3OH concentrations in the ices toward embedded stars show order-of-magnitude object-to-object variations, even in a sample restricted to stars of low mass associated with ices lacking evidence of thermal processing. We hypothesize that the efficiency of CH3OH production in dense cores and protostellar envelopes is mediated by the degree of prior CO depletion.
C1 [Whittet, D. C. B.; Cook, A. M.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Troy, NY 12180 USA.
[Whittet, D. C. B.; Cook, A. M.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA.
[Cook, A. M.; Shenoy, S. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Herbst, Eric] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Herbst, Eric] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA.
[Herbst, Eric] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Chiar, J. E.] SETI Inst, Mountain View, CA 94043 USA.
RP Whittet, DCB (reprint author), Rensselaer Polytech Inst, New York Ctr Astrobiol, 110 8th St, Troy, NY 12180 USA.
OI Whittet, Douglas/0000-0001-8539-3891
FU NASA [NNX11AG44G]; NASA Astrobiology Institute [NNA09DA80A]; National
Science Foundation [AST-0702876]; NASA through Rensselaer Polytechnic
Institute
FX D.C.B.W. acknowledges financial support from the NASA Exobiology and
Evolutionary Biology program (grant NNX11AG44G) and the NASA
Astrobiology Institute (grant NNA09DA80A). E. H. acknowledges support
from the National Science Foundation for his astrochemistry program
through grant AST-0702876, and support from the NASA Exobiology and
Evolutionary Biology program through a subcontract from Rensselaer
Polytechnic Institute. S. S. S. acknowledges receipt of a NASA
Postdoctoral Fellowship. We are grateful to Ewine van Dishoeck and an
anonymous referee for helpful comments.
NR 70
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U1 1
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
VL 742
IS 1
AR 28
DI 10.1088/0004-637X/742/1/28
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400028
ER
PT J
AU Marcu, DM
Furst, F
Pottschmidt, K
Grinberg, V
Muller, S
Wilms, J
Postnov, KA
Corbet, RHD
Markwardt, CB
Bel, MC
AF Marcu, Diana M.
Fuerst, Felix
Pottschmidt, Katja
Grinberg, Victoria
Mueller, Sebastian
Wilms, Joern
Postnov, Konstantin A.
Corbet, Robin H. D.
Markwardt, Craig B.
Cadolle Bel, Marion
TI THE 5 hr PULSE PERIOD AND BROADBAND SPECTRUM OF THE SYMBIOTIC X-RAY
BINARY 3A 1954+319
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: symbiotic; stars: individual (3A 1954+319); stars: neutron;
X-rays: binaries
ID LONG-PERIOD; CATALOG; 4U-1954+319; CYGNUS-X-1; 4U-1700+24; MISSION;
GX-1+4; GIANTS; STARS; BAT
AB We present an analysis of the highly variable accreting X-ray pulsar 3A 1954 + 319 using 2005-2009 monitoring data obtained with INTEGRAL and Swift. This considerably extends the pulse period history and covers flaring episodes in 2005 and 2008. In 2006 the source was identified as one of only a few known symbiotic X-ray binaries (SyXBs), i.e., systems composed of a neutron star accreting from the inhomogeneous medium around an M-giant star. The extremely long pulse period of similar to 5.3 hr is directly visible in the 2008 INTEGRAL-ISGRI outburst light curve. The pulse profile is double peaked and generally not significantly energy dependent although there is an indication of possible softening during the main pulse. During the outburst a strong spin-up of -1.8 x 10(-4) hr hr(-1) occurred. Between 2005 and 2008 a long-term spin-down trend of 2.1 x 10(-5) hr hr(-1) was observed for the first time for this source. The 3-80 keV pulse peak spectrum of 3A 1954 + 319 during the 2008 flare could be well described by a thermal Comptonization model. We interpret the results within the framework of a recently developed quasi-spherical accretion model for SyXBs.
C1 [Marcu, Diana M.; Pottschmidt, Katja; Corbet, Robin H. D.; Markwardt, Craig B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Marcu, Diana M.; Pottschmidt, Katja; Corbet, Robin H. D.] CRESST, Baltimore, MD 21250 USA.
[Marcu, Diana M.; Pottschmidt, Katja; Corbet, Robin H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Fuerst, Felix; Grinberg, Victoria; Mueller, Sebastian; Wilms, Joern] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Fuerst, Felix; Grinberg, Victoria; Mueller, Sebastian; Wilms, Joern] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
[Postnov, Konstantin A.] Moscow M V Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Cadolle Bel, Marion] European Space Agcy, European Space Astron Ctr, Madrid 28692, Spain.
RP Marcu, DM (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA.
RI Wilms, Joern/C-8116-2013
OI Wilms, Joern/0000-0003-2065-5410
FU NASA [NNX08AE84G, NNX08AY24G, NNX09AT28G]; DAAD; RFBR [10-02-00599];
European Commission, "Black Hole Universe" [ITN215212];
Bundesministerium fur Wirtschaft and Technologie [50OR0808, 50OR1007];
ESA, Denmark; ESA, France; ESA, Germany; ESA, Italy; ESA, Switzerland;
ESA, Spain
FX We thank the anonymous referee for useful comments. D.M.M. and K.P.
acknowledge NASA grants NNX08AE84G, NNX08AY24G, and NNX09AT28G. F.F.
acknowledges support from the DAAD and thanks the NASA-GSFC for its
hospitality. The work by K.A.P. is partially supported through RFBR
grant 10-02-00599. This research has been partly funded by the European
Commission under contract ITN215212 "Black Hole Universe" and by the
Bundesministerium fur Wirtschaft and Technologie under DLR grants
50OR0808 and 50OR1007. It is based on observations with INTEGRAL, an ESA
project with instruments and science data centre funded by ESA member
states (especially the PI countries: Denmark, France, Germany, Italy,
Switzerland, Spain), Czech Republic, and Poland, and with the
participation of Russia and the USA. We thank the INTEGRAL mission
planners for careful scheduling of the Cygnus region Key Program. We
also thank Hans Krimm and the Swift-BAT team for making the Swift-BAT
light curves available.
NR 42
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U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 20
PY 2011
VL 742
IS 1
AR L11
DI 10.1088/2041-8205/742/1/L11
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QY
UT WOS:000296763600011
ER
PT J
AU Monnier, JD
Zhao, M
Pedretti, E
Millan-Gabet, R
Berger, JP
Traub, W
Schloerb, FP
ten Brummelaar, T
McAlister, H
Ridgway, S
Sturmann, L
Sturmann, J
Turner, N
Baron, F
Kraus, S
Tannirkulam, A
Williams, PM
AF Monnier, J. D.
Zhao, Ming
Pedretti, E.
Millan-Gabet, R.
Berger, J. -P.
Traub, W.
Schloerb, F. P.
ten Brummelaar, T.
McAlister, H.
Ridgway, S.
Sturmann, L.
Sturmann, J.
Turner, N.
Baron, F.
Kraus, S.
Tannirkulam, A.
Williams, P. M.
TI FIRST VISUAL ORBIT FOR THE PROTOTYPICAL COLLIDING-WIND BINARY WR 140
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: visual; infrared: stars; stars: individual (WR 140, HD
193793); stars: Wolf-Rayet; techniques: interferometric
ID WOLF-RAYET STARS; GALACTIC-O-STARS; RADIO OBSERVATIONS; LAMBDA-VIRGINIS;
DUST FORMATION; INTERFEROMETRY; PHOTOMETRY; CATALOG; MODELS; IOTA
AB Wolf-Rayet (WR) stars represent one of the final stages of massive stellar evolution. Relatively little is known about this short-lived phase and we currently lack reliable mass, distance, and binarity determinations for a representative sample. Here we report the first visual orbit for WR 140 (=HD193793), a WC7+O5 binary system known for its periodic dust production episodes triggered by intense colliding winds near periastron passage. The Infrared-Optical Telescope Array and Center for High Angular Resolution Astronomy interferometers resolved the pair of stars in each year from 2003 to 2009, covering most of the highly eccentric, 7.9 year orbit. Combining our results with the recently improved double-line spectroscopic orbit of Fahed et al., we find the WR 140 system is located at a distance of 1.67 +/- 0.03 kpc, composed of a WR star with M(WR) = 14.9 +/- 0.5 M(circle dot) and an O star with M(O) = 35.9 +/- 1.3 M(circle dot). Our precision orbit yields key parameters with uncertainties similar to 6x smaller than previous work and paves the way for detailed modeling of the system. Our newly measured flux ratios at the near-infrared H and Ks bands allow a spectral energy distribution decomposition and analysis of the component evolutionary states.
C1 [Monnier, J. D.; Zhao, Ming; Pedretti, E.; Baron, F.; Kraus, S.; Tannirkulam, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Pedretti, E.] European Org Astron Res So Hemisphere, D-85748 Garching, Germany.
[Millan-Gabet, R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Berger, J. -P.] Univ Grenoble 1, CNRS, UMR 5571, IPAG, F-38041 Grenoble, France.
[Traub, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schloerb, F. P.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[ten Brummelaar, T.; McAlister, H.; Sturmann, L.; Sturmann, J.; Turner, N.] Georgia State Univ, CHARA Array, Mt Wilson, CA 91023 USA.
[Ridgway, S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Tannirkulam, A.] Inst Financial Management & Res, Ctr Micro Finance, Chennai 600113, Tamil Nadu, India.
[Williams, P. M.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh, Midlothian, Scotland.
RP Monnier, JD (reprint author), Univ Michigan, Dept Astron, 941 Dennison Bldg, Ann Arbor, MI 48109 USA.
EM monnier@umich.edu
FU SAO, U. Mass, NSF [AST-0138303]; NSF [AST-0352723, AST-0908253,
AST-0807577]; NASA [NNG05G1180G]; GSU; Keck Foundation; CNRS; CNES
(France); Michelson Postdoctoral Fellowship; Scottish Universities
Physics Alliance (SUPA)
FX We have appreciated discussions with Tony Moffat, Peter Tuthill, Debra
Wallace, Bill Danchi, Sean Dougherty, and Remi Fahed during the (long)
course of this work. We thank SAO, U. Mass, NSF AST-0138303, NSF
AST-0352723, and NASA NNG05G1180G for supporting IOTA development and
operations. We also acknowledge funding from GSU, the Keck Foundation,
and NSF AST-0908253 for the CHARA Array. IONIC-3 was developed by LAOG
(now IPAG) and LETI in the context of the IONIC collaboration (LAOG,
IMEP, LETI), funded by the CNRS and CNES (France). Lastly we thank NSF
AST-0807577 for support of University of Michigan researchers in this
work. E.P. received funding from a Michelson Postdoctoral Fellowship and
a Scottish Universities Physics Alliance (SUPA) advanced fellowship.
P.M.W. is grateful to the Institute for Astronomy for hospitality and
continued access to the facilities of the Royal Observatory, Edinburgh.
This research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France, and NASA's Astrophysics Data System (ADS)
Bibliographic Services.
NR 32
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U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 20
PY 2011
VL 742
IS 1
AR L1
DI 10.1088/2041-8205/742/1/L1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QY
UT WOS:000296763600001
ER
PT J
AU Mulu-Moore, FM
Winebarger, AR
Warren, HP
AF Mulu-Moore, Fana M.
Winebarger, Amy R.
Warren, Harry P.
TI CAN A LONG NANOFLARE STORM EXPLAIN THE OBSERVED EMISSION MEASURE
DISTRIBUTIONS IN ACTIVE REGION CORES?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona
ID EXTREME-ULTRAVIOLET OBSERVATIONS; TRANSITION-REGION; CORONAL LOOPS;
X-RAY; SIMULATIONS; CONSTRAINTS; EXPLORER; HINODE; TRACE; MOSS
AB All theories that attempt to explain the heating of the high-temperature plasma observed in the solar corona are based on short bursts of energy. The intensities and velocities measured in the cores of quiescent active regions, however, can be steady over many hours of observation. One heating scenario that has been proposed to reconcile such observations with impulsive heating models is the "long nanoflare storm," where short-duration heating events occur infrequently on many sub-resolution strands; the emission of the strands is then averaged together to explain the observed steady structures. In this Letter, we examine the emission measure distribution predicted for such a long nanoflare storm by modeling an arcade of strands in an active region core. Comparisons of the computed emission measure distributions with recent observations indicate that the long nanoflare storm scenario implies greater than five times more 1 MK emission than is actually observed for all plausible combinations of loop lengths, heating rates, and abundances. We conjecture that if the plasma had "super coronal" abundances, the model may be able to match the observations at low temperatures.
C1 [Mulu-Moore, Fana M.; Winebarger, Amy R.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Warren, Harry P.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
RP Mulu-Moore, FM (reprint author), NASA, Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA.
EM fanamariam.mulumoore@nasa.gov
FU NASA
FX The author, F.M.M., is supported by an appointment to NASA's
Postdoctoral Program (NPP) which is administered by Oak Ridge Associated
Universities (ORAU). The authors thank the NPP host facility, Marshall
Space Flight Center, and are also grateful to the referee for providing
helpful comments to improve the manuscript.
NR 30
TC 11
Z9 11
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 20
PY 2011
VL 742
IS 1
AR L6
DI 10.1088/2041-8205/742/1/L6
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QY
UT WOS:000296763600006
ER
PT J
AU White, TR
Bedding, TR
Stello, D
Appourchaux, T
Ballot, J
Benomar, O
Bonanno, A
Broomhall, AM
Campante, TL
Chaplin, WJ
Christensen-Dalsgaard, J
Corsaro, E
Dogan, G
Elsworth, YP
Fletcher, ST
Garcia, RA
Gaulme, P
Handberg, R
Hekker, S
Huber, D
Karoff, C
Kjeldsen, H
Mathur, S
Mosser, B
Monteiro, MJPFG
Regulo, C
Salabert, D
Aguirre, VS
Thompson, MJ
Verner, G
Morris, RL
Sanderfer, DT
Seader, SE
AF White, Timothy R.
Bedding, Timothy R.
Stello, Dennis
Appourchaux, Thierry
Ballot, Jerome
Benomar, Othman
Bonanno, Alfio
Broomhall, Anne-Marie
Campante, Tiago L.
Chaplin, William J.
Christensen-Dalsgaard, Jorgen
Corsaro, Enrico
Dogan, Gulnur
Elsworth, Yvonne P.
Fletcher, Stephen T.
Garcia, Rafael A.
Gaulme, Patrick
Handberg, Rasmus
Hekker, Saskia
Huber, Daniel
Karoff, Christoffer
Kjeldsen, Hans
Mathur, Savita
Mosser, Benoit
Monteiro, Mario J. P. F. G.
Regulo, Clara
Salabert, David
Aguirre, Victor Silva
Thompson, Michael J.
Verner, Graham
Morris, Robert L.
Sanderfer, Dwight T.
Seader, Shawn E.
TI ASTEROSEISMIC DIAGRAMS FROM A SURVEY OF SOLAR-LIKE OSCILLATIONS WITH
KEPLER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: oscillations
ID MODE FREQUENCIES; RED GIANTS; STARS; COROT; SUN; PARAMETERS; PIPELINE;
SPECTRUM; SCIENCE; MISSION
AB Photometric observations made by the NASA Kepler Mission have led to a dramatic increase in the number of main-sequence and subgiant stars with detected solar-like oscillations. We present an ensemble asteroseismic analysis of 76 solar-type stars. Using frequencies determined from the Kepler time-series photometry, we have measured three asteroseismic parameters that characterize the oscillations: the large frequency separation (Delta nu), the small frequency separation between modes of l = 0 and l = 2 (delta nu(02)), and the dimensionless offset (epsilon). These measurements allow us to construct asteroseismic diagrams, namely the so-called Christensen-Dalsgaard diagram of delta nu(02) versus Delta nu, and the recently re-introduced epsilon diagram. We compare the Kepler results with previously observed solar-type stars and with theoretical models. The positions of stars in these diagrams places constraints on their masses and ages. Additionally, we confirm the observational relationship between epsilon and T-eff that allows for the unambiguous determination of radial order and should help resolve the problem of mode identification in F stars.
C1 [White, Timothy R.; Bedding, Timothy R.; Stello, Dennis; Benomar, Othman; Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[White, Timothy R.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Appourchaux, Thierry; Benomar, Othman; Gaulme, Patrick] Univ Paris 11, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Ballot, Jerome] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Ballot, Jerome] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
[Bonanno, Alfio; Corsaro, Enrico] INAF Observ Astrofis Catania, I-95123 Catania, Italy.
[Broomhall, Anne-Marie; Chaplin, William J.; Elsworth, Yvonne P.; Hekker, Saskia; Verner, Graham] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Campante, Tiago L.; Monteiro, Mario J. P. F. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Campante, Tiago L.; Christensen-Dalsgaard, Jorgen; Dogan, Gulnur; Handberg, Rasmus; Karoff, Christoffer; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, Danish AsteroSeismol Ctr DASC, DK-8000 Aarhus C, Denmark.
[Campante, Tiago L.; Monteiro, Mario J. P. F. G.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
[Fletcher, Stephen T.] Sheffield Hallam Univ, Fac Arts Comp Engn & Sci, Mat Engn Res Inst, Sheffield S1 1WB, S Yorkshire, England.
[Garcia, Rafael A.] Univ Paris 07, Ctr Saclay, IRFU SAp, CEA DSM CNRS,Lab AIM, F-91191 Gif Sur Yvette, France.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Mathur, Savita; Thompson, Michael J.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Mosser, Benoit] Univ Paris 07, Univ Paris 06, Observ Paris, CNRS,LESIA, F-92195 Meudon, France.
[Regulo, Clara] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Regulo, Clara] Univ la Laguna, Dept Astrofis, E-38206 San Cristobal de la Laguna, Spain.
[Salabert, David] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France.
[Aguirre, Victor Silva] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Verner, Graham] Queen Mary Univ London, Sch Math Sci, Astron Unit, London E1 4NS, England.
[Morris, Robert L.; Seader, Shawn E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP White, TR (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
EM t.white@physics.usyd.edu.au
RI Ballot, Jerome/G-1019-2010; Monteiro, Mario J.P.F.G./B-4715-2008;
OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Bonanno,
Alfio/0000-0003-3175-9776; Bedding, Timothy/0000-0001-5943-1460; Karoff,
Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661;
Garcia, Rafael/0000-0002-8854-3776; Handberg, Rasmus/0000-0001-8725-4502
FU NASA's Science Mission Directorate; Australian Postgraduate Award;
University of Sydney; Australian Astronomical Observatory PhD
Scholarship; Denison Merit Award; Australian Research Council;
Netherlands Organisation for Scientific Research; Spanish National
Research Plan [AYA2010-17803]; National Science Foundation
FX The authors gratefully acknowledge the Kepler Science Team and all those
who have contributed to the Kepler Mission for their tireless efforts
which have made these results possible. Funding for the Kepler Mission
is provided by NASA's Science Mission Directorate. T.R.W. is supported
by an Australian Postgraduate Award, a University of Sydney Merit Award,
an Australian Astronomical Observatory PhD Scholarship, and a Denison
Merit Award. T.R.B. and D.S. acknowledge the support of the Australian
Research Council. S.H. acknowledges financial support from The
Netherlands Organisation for Scientific Research. This research was
supported by grant AYA2010-17803 from the Spanish National Research
Plan. NCAR is supported by the National Science Foundation.
NR 50
TC 23
Z9 23
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 20
PY 2011
VL 742
IS 1
AR L3
DI 10.1088/2041-8205/742/1/L3
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QY
UT WOS:000296763600003
ER
PT J
AU Wiese, DN
Nerem, RS
Han, SC
AF Wiese, David N.
Nerem, Robert S.
Han, Shin-Chan
TI Expected improvements in determining continental hydrology, ice mass
variations, ocean bottom pressure signals, and earthquakes using two
pairs of dedicated satellites for temporal gravity recovery
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID LOCALIZED SPECTRAL-ANALYSIS; CLIMATE EXPERIMENT; FIELD MODELS; GLOBAL
OCEAN; GRACE; MISSION; TIDES; ASSIMILATION; VARIABILITY; DESIGN
AB The Gravity Recovery and Climate Experiment mission has demonstrated the ability to quantify global mass variations at large spatial scales with monthly to sub-monthly temporal resolution. Future missions of this type taking advantage of improved measurement technologies will be limited by temporal aliasing errors. We suggest the addition of a second pair of satellites to reduce these errors. Using an optimized mission architecture consisting of a polar pair of satellites coupled with a lower inclined pair of satellites (72 degrees), both in 13-day repeating orbits, we quantify the expected scientific improvements that having two pairs of satellites will provide over one pair. Numerical simulations to spherical harmonic degree 100 are run over one full year. Analysis using empirical orthogonal functions reveals that two satellite pairs determine annual mass variations in small basins which are undetected using one pair of satellites. Averaging kernels are used to show that two satellite pairs offer an 80% reduction in the level of error in determining mass variations in 53 hydrological basins and 12 Greenland basins over the year. After standard GRACE post-processing techniques have been applied to the one-pair solutions, it is seen that two satellite pairs (with no post-processing) still offer a 25%-75% improvement in determining the mass variations. Spatiospectral localization analysis is used to show increased spatial resolution and higher signal-to-noise ratios in recovering hydrology in the Amazon River basin, ocean bottom pressure signals in the Southeast Pacific basin, and a simulated earthquake signal representative of the 2010 Maule, Chile earthquake.
C1 [Wiese, David N.; Nerem, Robert S.] Univ Colorado, Colorado Ctr Astrodynam Res, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Nerem, Robert S.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO USA.
[Han, Shin-Chan] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wiese, DN (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, Dept Aerosp Engn Sci, 431 UCB, Boulder, CO 80309 USA.
EM wiese@colorado.edu; nerem@colorado.edu; shin-chan.han@nasa.gov
RI Han, Shin-Chan/A-2022-2009
FU National Science Foundation; National Defense Science and Engineering
Graduate Fellowship Program; NASA GRACE Science Team investigation
[NNX08AH63G]
FX This research was funded by the National Science Foundation Graduate
Fellowship Program, the National Defense Science and Engineering
Graduate Fellowship Program, and the NASA GRACE Science Team
investigation (NNX08AH63G). The authors would like to thank NASA Goddard
Space Flight Center for providing GEODYN and SOLVE to perform the
numerical simulations, along with the NCEP model. We acknowledge
Jean-Paul Boy (EOST/University of Strasbourg, France) for providing the
ECMWF-derived and MOG-2D-derived data sets in this study to GSFC.
Additionally, we thank the European Space Agency (ESA) and the Institute
of Astronomical and Physical Geodesy (IAPG) at the Technical University
of Munich for providing the ice model used in the simulations. Jianli
Chen from the Center for Space Research at the University of Texas at
Austin is acknowledged for providing the hydrology basin definitions
while Bryant Loomis of SGT is acknowledged for providing the Greenland
basin definitions.
NR 61
TC 5
Z9 5
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD NOV 19
PY 2011
VL 116
AR B11405
DI 10.1029/2011JB008375
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 851HB
UT WOS:000297257900001
ER
PT J
AU Sun, WB
Videen, G
Kato, S
Lin, B
Lukashin, C
Hu, YX
AF Sun, Wenbo
Videen, Gorden
Kato, Seiji
Lin, Bing
Lukashin, Constantine
Hu, Yongxiang
TI A study of subvisual clouds and their radiation effect with a synergy of
CERES, MODIS, CALIPSO, and AIRS data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CIRRUS CLOUDS; TROPICAL TROPOPAUSE; WATER-VAPOR; AEROSOLS; MISSION;
ENERGY; LIDAR; THIN; OCEANS
AB Subvisual cirrus clouds that are defined as those whose optical thickness is less than similar to 0.3 are found in similar to 50% of global observations. Passive remote-sensing instruments, such as the Moderate Resolution Imaging Spectroradiometer (MODIS), generally fail to detect these optically thin clouds. The launch of NASA's Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) satellite provides an unprecedented ability to detect thin cloud layers globally. Also, the Clouds and the Earth's Radiant Energy System (CERES) provides accurate measurements of top-of-atmosphere radiation. By using CERES, MODIS, and CALIPSO measurements in a synergistic manner, a quantitative assessment of the influence of subvisual clouds on the Earth's shortwave (SW) radiation is accomplished. The difference between clear-sky radiation flux and the flux obtained with the presence of subvisual clouds clearly shows the cooling effect of subvisual clouds in the SW. The subvisual clouds increase the diurnal mean reflected SW flux by similar to 2.5 W m(-2). The subvisual clouds' effect on outgoing longwave radiation is also studied using a radiative-transfer model. The model results show that a layer of subvisual clouds having optical thickness of 0.1 can have a warming effect of similar to 15 W m(-2). These clouds can also affect the polarization of the reflected SW radiation and the accuracy of aerosol retrieval with satellite measurements. This work demonstrates that the study of subvisual clouds is necessary for an accurate and detailed understanding of Earth-atmosphere radiation.
C1 [Sun, Wenbo; Kato, Seiji; Lin, Bing; Lukashin, Constantine; Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Videen, Gorden] Space Sci Inst, Boulder, CO 80301 USA.
[Sun, Wenbo] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Sun, WB (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA.
EM wenbo.sun-1@nasa.gov
RI Hu, Yongxiang/K-4426-2012; Richards, Amber/K-8203-2015
FU NASA CERES; CLARREO Missions; NASA [09-GLORY09-0027]
FX This work was partially supported by NASA CERES and CLARREO Missions.
This work was also supported by NASA Glory fund 09-GLORY09-0027. The
authors thank Bruce A. Wielicki, Norman G. Loeb, Dave F. Young, Michael
I. Mishchenko, and Hal B. Maring for their support of this work. The
authors also thank Shana Mattoo for help with using the MOD04 data.
NR 31
TC 23
Z9 23
U1 4
U2 22
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 NOV 19
PY 2011
VL 116
AR D22207
DI 10.1029/2011JD016422
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 851KP
UT WOS:000297268300009
ER
PT J
AU Simard, M
Pinto, N
Fisher, JB
Baccini, A
AF Simard, Marc
Pinto, Naiara
Fisher, Joshua B.
Baccini, Alessandro
TI Mapping forest canopy height globally with spaceborne lidar
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID ABOVEGROUND BIOMASS; VERTICAL STRUCTURE; CARBON STOCKS; VEGETATION
STRUCTURE; TEMPERATE FOREST; NEW-HAMPSHIRE; ICESAT; VALIDATION; DIOXIDE;
LESSONS
AB Data from spaceborne light detection and ranging (lidar) opens the possibility to map forest vertical structure globally. We present a wall-to-wall, global map of canopy height at 1-km spatial resolution, using 2005 data from the Geoscience Laser Altimeter System (GLAS) aboard ICESat (Ice, Cloud, and land Elevation Satellite). A challenge in the use of GLAS data for global vegetation studies is the sparse coverage of lidar shots (mean = 121 data points/degree(2) for the L3C campaign). However, GLAS-derived canopy height (RH100) values were highly correlated with other, more spatially dense, ancillary variables available globally, which allowed us to model global RH100 from forest type, tree cover, elevation, and climatology maps. The difference between the model predicted RH100 and footprint level lidar-derived RH100 values showed that error increased in closed broadleaved forests such as the Amazon, underscoring the challenges in mapping tall (>40 m) canopies. The resulting map was validated with field measurements from 66 FLUXNET sites. The modeled RH100 versus in situ canopy height error (RMSE = 6.1 m, R-2 = 0.5; or, RMSE = 4.4 m, R-2 = 0.7 without 7 outliers) is conservative as it also includes measurement uncertainty and sub pixel variability within the 1-km pixels. Our results were compared against a recently published canopy height map. We found our values to be in general taller and more strongly correlated with FLUXNET data. Our map reveals a global latitudinal gradient in canopy height, increasing towards the equator, as well as coarse forest disturbance patterns.
C1 [Simard, Marc; Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Baccini, Alessandro] Woods Hole Res Ctr, Falmouth, MA 02540 USA.
[Pinto, Naiara] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
RP Simard, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM marc.simard@jpl.nasa.gov
RI Simard, Marc/H-3516-2013;
OI Simard, Marc/0000-0002-9442-4562; Fisher, Joshua/0000-0003-4734-9085
FU National Aeronautics and Space Administration; MEaSUREs program [WBS
547714.04.14.01.13]; NASA
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Funded through the MEaSUREs
program (project WBS 547714.04.14.01.13). N. Pinto was funded by the
NASA Postdoctoral Program (NPP). The authors would like to thank
fruitful discussions with Claudia Carabajal, Mike Kobrick, Ralph Dubayah
as well as the anonymous reviewers for their constructive comments. M.
Simard is funded by the NASA MEaSUREs program. Canopy height data were
provided to J. Fisher by the PI's part of FLUXNET.
NR 36
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Z9 183
U1 9
U2 84
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD NOV 19
PY 2011
VL 116
AR G04021
DI 10.1029/2011JG001708
PG 12
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 851IE
UT WOS:000297260900001
ER
PT J
AU Cooper, OR
Oltmans, SJ
Johnson, BJ
Brioude, J
Angevine, W
Trainer, M
Parrish, DD
Ryerson, TR
Pollack, I
Cullis, PD
Ives, MA
Tarasick, DW
Al-Saadi, J
Stajner, I
AF Cooper, O. R.
Oltmans, S. J.
Johnson, B. J.
Brioude, J.
Angevine, W.
Trainer, M.
Parrish, D. D.
Ryerson, T. R.
Pollack, I.
Cullis, P. D.
Ives, M. A.
Tarasick, D. W.
Al-Saadi, J.
Stajner, I.
TI Measurement of western US baseline ozone from the surface to the
tropopause and assessment of downwind impact regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TRANSPORTED BACKGROUND OZONE; MARINE BOUNDARY-LAYER; LONG-RANGE
TRANSPORT; ASIAN AIR-POLLUTION; UNITED-STATES; NORTH-AMERICA;
INTERANNUAL VARIABILITY; TROPOSPHERIC OZONE; CALIFORNIA OZONE;
CARBON-MONOXIDE
AB Since 1997, baseline ozone monitoring from the surface to the tropopause along the U. S. west coast has been limited to the weekly ozonesondes from Trinidad Head, California. To explore baseline ozone at other latitudes, an ozonesonde network was implemented during spring 2010, including four launch sites along the California coast. Modeling indicated that North American pollution plumes impacted the California coast primarily below 3 km, but had no measurable impact on the average coastal ozone profiles. Vertical and latitudinal variation in free tropospheric baseline ozone appears to be partly explained by polluted and stratospheric air masses that descend isentropically along the west coast. Above 3 km, the dominant sources of ozone precursors were China and international shipping, while international shipping was the greatest source below 2 km. Approximately 8-10% of the baseline ozone that enters California in the 0-6 km range impacts the surface of the USA, but very little reaches the eastern USA. Within California, the major impact of baseline ozone above 2 km is on the high elevation terrain of eastern California. Baseline ozone below 2 km has its strongest impact on the low elevation sites throughout the state. To quantify ozone production within California we compared inland ozone measurements to baseline measurements. For average daytime conditions, we found no enhancements of lower tropospheric ozone in the northern Central Valley, but enhancements of 12-23% were found in the southern Central Valley. Enhancements above Joshua Tree were greater, 33-41%, while the greatest enhancements occurred over the LA Basin, 32-63%.
C1 [Cooper, O. R.; Oltmans, S. J.; Brioude, J.; Angevine, W.; Pollack, I.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80305 USA.
[Al-Saadi, J.] NASA, Tropospher Chem Program, Div Earth Sci, Sci Mission Directorate, Washington, DC 20546 USA.
[Cooper, O. R.; Oltmans, S. J.; Johnson, B. J.; Brioude, J.; Angevine, W.; Trainer, M.; Parrish, D. D.; Ryerson, T. R.; Pollack, I.; Cullis, P. D.] NOAA, Earth Syst Res Lab, Boulder, CO 80304 USA.
[Ives, M. A.] NOAA, Trinidad Head Observ, ESRL, HSU Marine Lab, Trinidad Head, CA 95570 USA.
[Stajner, I.] NOAA, Off Sci & Technol, Natl Weather Serv, Silver Spring, MD 20910 USA.
[Tarasick, D. W.] Environm Canada, Expt Studies Res Div, MSC, Downsview, ON M3H 5T4, Canada.
[Stajner, I.] Noblis, Falls Church, VA USA.
RP Cooper, OR (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, 325 Broadway, Boulder, CO 80305 USA.
EM owen.cooper@colorado.edu
RI Ryerson, Tom/C-9611-2009; Angevine, Wayne/H-9849-2013; Manager, CSD
Publications/B-2789-2015; Parrish, David/E-8957-2010; Brioude,
Jerome/E-4629-2011; Pollack, Ilana/F-9875-2012; Stajner,
Ivanka/B-5228-2009; Cooper, Owen/H-4875-2013; Trainer,
Michael/H-5168-2013
OI Angevine, Wayne/0000-0002-8021-7116; Tarasick,
David/0000-0001-9869-0692; Parrish, David/0000-0001-6312-2724; Stajner,
Ivanka/0000-0001-6103-3939;
FU NOAA ESRL; NASA; U.S. Navy; Environment Canada; NOAA's National Air
Quality Forecast Capability
FX Funding for the IONS-2010 field campaign was provided by NOAA ESRL
Health of the Atmosphere Program, NASA Tropospheric Chemistry Program,
U.S. Navy, Environment Canada, and NOAA's National Air Quality Forecast
Capability. We are extremely grateful for the efforts of the IONS-2010
ozonesonde operators who made this study a success: Michael Parrish at
Point Reyes, Chance Sterling and Rigeto Zhao at Shasta, Lauren Hayduk at
Trinidad Head, Lee Eddington and Matthew McGovern at Point Sur, Robert
Nagy, Joel Guerrero and Kyle Edwards at San Nicolas Island, and Afeworki
Mekonnen at Kelowna. We also thank Emrys Hall and Allen Jordan at NOAA
ESRL GMD for the use of the Skysonde software and for their assistance
in processing the Joshua Tree ozonesondes. We truly appreciate our
collaboration with John D. Ray at the National Park Service Air
Resources Division, Denver, Colorado, who helped us gain permission to
collect data in the National Parks. Operations were also facilitated by
the excellent support we received from the staff of the National Parks
and California State Parks: Luke Sabala and Victoria Chang at Joshua
Tree National Park; William Shook and Ben Becker at Point Reyes National
Seashore; Heidi Horvitz and Lori Martin at Shasta State Historic Park;
and C. L. Price at Point Sur State Historic Park. Chris Miller and Dick
Lind from the Naval Postgraduate School (NPS), Monterey, were extremely
helpful in allowing us to launch the Point Sur ozonesondes from NPS
property. Finally we thank Carol Long with the Federal Aviation
Administration for helping coordinate the ozonesonde launch schedule
with air traffic controllers. The EDGARv4.1 global NOx
emissions inventory was provided by European Commission, Joint Research
Centre (JRC)/Netherlands Environmental Assessment Agency (PBL): Emission
Database for Global Atmospheric Research (EDGAR), release version 4.1
http://edgar.jrc.ec.europa.eu, 2010. The international shipping NOx
emission inventory was provided by James Corbett, University of
Delaware. Fire NOx emissions are from the Global Fire Emissions Database
version 3 (GFED3). The global land cover data set, as well as the MODIS
fire detection data, was provided by the University of Maryland MODIS
Active Fire and Burned Area Products from their ftp server. NCEP
reanalysis data were provided by the NOAA/ESRL Physical Sciences
Division, Boulder, Colorado from their web site:
http://www.esrl.noaa.gov/psd/
NR 73
TC 37
Z9 38
U1 2
U2 44
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 NOV 18
PY 2011
VL 116
AR D00V03
DI 10.1029/2011JD016095
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 851KO
UT WOS:000297268100003
ER
PT J
AU Goswami, BB
Mani, NJ
Mukhopadhyay, P
Waliser, DE
Benedict, JJ
Maloney, ED
Khairoutdinov, M
Goswami, BN
AF Goswami, Bidyut B.
Mani, Neena Joseph
Mukhopadhyay, P.
Waliser, Duane E.
Benedict, James J.
Maloney, Eric D.
Khairoutdinov, Marat
Goswami, B. N.
TI Monsoon intraseasonal oscillations as simulated by the
superparameterized Community Atmosphere Model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ASIAN SUMMER MONSOON; CLOUD-RESOLVING MODEL; MADDEN-JULIAN OSCILLATION;
SUBSEASONAL VARIABILITY; CLIMATE MODELS; RESOLUTION; WAVES; GCM;
PREDICTABILITY; PRECIPITATION
AB The relative success of the Community Atmosphere Model with superparameterized convection (SP-CAM) in simulating the space-time characteristics of the Madden Julian Oscillation encourages us to examine its simulation of the Indian summer monsoon and monsoon intraseasonal oscillations (MISOs). While the model simulates the onset and withdrawal of the Indian monsoon realistically, it has a significant wet bias in boreal summer precipitation over the Asian monsoon region. The space-time characteristics of the MISOs simulated by the SP-CAM are examined in detail and compared with those of the observed MISO to gain insight into the model's bias in simulating the seasonal mean. During northern summer, the model simulates a 20 day mode and a 60 day mode in place of the observed 15 and 45 day modes, respectively. The simulated 20 day mode appears to have no observed analog with a baroclinic vertical structure and strong northward propagation over Indian longitudes. The simulated 60 day mode seems to be a lower-frequency version of the observed 45 day mode with relatively slower northward propagation. The model's underestimation of light rain events and overestimation of heavy rain events are shown to be responsible for the wet bias of the model. More frequent occurrence of heavy rain events in the model is, in turn, related to the vertical structure of the higher-frequency modes. Northward propagation of the simulated 20 day mode is associated with a strong cyclonic vorticity at low levels north of the heating maximum associated with a smaller meridional scale of the simulated mode. The simulated vertical structure of heating indicates a strong maximum in the upper troposphere between 200 and 300 hPa. Such a heating profile seems to generate a higher-order baroclinic mode response with smaller meridional structure, stronger low-level cyclonic vorticity, enhanced low-level moisture convergence, and higher precipitation. Therefore, the vertical structure of heating simulated by the cloud-resolving model within SP-CAM may hold the key for improving the precipitation bias in the model.
C1 [Goswami, Bidyut B.; Mani, Neena Joseph; Mukhopadhyay, P.; Goswami, B. N.] Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India.
[Benedict, James J.; Maloney, Eric D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Khairoutdinov, Marat] SUNY Stony Brook, Sch Marine & Atmospher Sci, New York, NY 11794 USA.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Goswami, BB (reprint author), Indian Inst Trop Meteorol, Dr Homi Bhabha Rd, Pune 411008, Maharashtra, India.
EM mpartha@tropmet.res.in
RI Benedict, James/M-5824-2013; Maloney, Eric/A-9327-2008;
OI Benedict, James/0000-0001-5115-5131; Maloney, Eric/0000-0002-2660-2611;
Goswami, Bidyut Bikash/0000-0001-8602-3083
FU Ministry of Earth Sciences, Government of India, New Delhi; National
Science Foundation [ATM-0832868, AGS-1025584]; Science and Technology
Center for MultiScale Modeling of Atmospheric Processes [ATM-0425247];
National Oceanic and Atmospheric Administration, U.S. Department of
Commerce [NA08OAR4320893]; National Aeronautics and Space Administration
FX The Indian Institute of Tropical Meteorology (Pune, India) is fully
funded by the Ministry of Earth Sciences, Government of India, New
Delhi. Eric D. Maloney was supported by the Climate and Large-Scale
Dynamics Program of the National Science Foundation under grants
ATM-0832868 and AGS-1025584 and by the Science and Technology Center for
MultiScale Modeling of Atmospheric Processes, managed by Colorado State
University under cooperative agreement ATM-0425247. Eric D. Maloney and
James J. Benedict were also supported by award NA08OAR4320893 from the
National Oceanic and Atmospheric Administration, U.S. Department of
Commerce. The statements, findings, conclusions, and recommendations do
not necessarily reflect the views of the National Science Foundation
(NSF), NOAA, or the Department of Commerce. We thank the National Center
for Environmental Prediction (NCEP) for the reanalysis data used in this
paper. We thank David A. Randall (Department of Atmospheric Science,
Colorado State University (CSU)) for permitting us to use the model
output. We also thank Mark Branson (Department of Atmospheric Science,
CSU) and Daehyun Kim (Lamont-Doherty Earth Observatory of Columbia
University) for arranging the data access. The MJO CLIVAR working group
(http://climate.snu.ac.kr/mjo_diagnostics/index.htm) is acknowledged for
the diagnostics used in some of the figures. D.W.'s contribution to this
study was carried out on behalf of the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 46
TC 7
Z9 7
U1 0
U2 8
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 NOV 18
PY 2011
VL 116
AR D22104
DI 10.1029/2011JD015948
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 851KO
UT WOS:000297268100002
ER
PT J
AU Korth, H
Anderson, BJ
Raines, JM
Slavin, JA
Zurbuchen, TH
Johnson, CL
Purucker, ME
Winslow, RM
Solomon, SC
McNutt, RL
AF Korth, Haje
Anderson, Brian J.
Raines, Jim M.
Slavin, James A.
Zurbuchen, Thomas H.
Johnson, Catherine L.
Purucker, Michael E.
Winslow, Reka M.
Solomon, Sean C.
McNutt, Ralph L., Jr.
TI Plasma pressure in Mercury's equatorial magnetosphere derived from
MESSENGER Magnetometer observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; ELECTRIC-FIELDS; PARTICLE MOTION; SHEET
ACCESS; SOLAR-WIND; MODEL; MAGNETOTAIL; INSTRUMENT; CONVECTION; IONS
AB Since insertion of the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft into orbit around Mercury on 18 March 2011, the probe's Magnetometer has routinely observed localized reductions of the magnetic field magnitude below the level predicted by a planetary dipole model corrected for magnetospheric magnetic fields. These magnetic depressions are observed on almost every orbit, and the latitude at which they are observed is local-time dependent. The depression signatures are indicators of the presence of enhanced plasma pressures, which inflate the magnetic field locally to maintain pressure balance, thus lowering the magnetic flux density. Mapping the magnetic depressions in local time and latitude provides insight into the plasma distribution near the planet, which complements that provided by MESSENGER's Fast Imaging Plasma Spectrometer. The spatial distribution shows that magnetic depressions are concentrated in two distinct regions, one near the equator on the nightside and another at high latitudes principally on the dayside. Here we focus on the nightside, equatorial pressure signatures, which we attribute to the magnetotail plasma sheet. The plasma-sheet pressures extend from dusk to dawn and are offset northward from the planetary geographic equator by about 10 in latitude, commensurate with the offset of the planetary dipole. The pressures associated with the plasma-sheet depressions range from 0.1 to 3 nPa and are systematically higher at dawn than at dusk. Proton gradient-curvature and convection drift in Mercury's dipole magnetic field with a dawn-to-dusk electric field result in low drift velocities near dawn, leading to systematically higher densities and pressures at dawn than at dusk, consistent with the observations. Citation: Korth, H., B. J. Anderson, J. M. Raines, J. A. Slavin, T. H. Zurbuchen, C. L. Johnson, M. E. Purucker, R. M. Winslow, S. C. Solomon, and R. L. McNutt Jr. (2011), Plasma pressure inMercury's equatorial magnetosphere derived from MESSENGER Magnetometer observations, Geophys. Res. Lett., 38, L22201, doi:10.1029/2011GL049451.
C1 [Korth, Haje; Anderson, Brian J.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Johnson, Catherine L.; Winslow, Reka M.] Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada.
[Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ USA.
[Purucker, Michael E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Korth, H (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
EM haje.korth@jhuapl.edu
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166
FU NASA [NAS5-97271, NASW-00002]; NSERC
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to the Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington. CLJ
and RW acknowledge support from NSERC.
NR 34
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U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD NOV 17
PY 2011
VL 38
AR L22201
DI 10.1029/2011GL049451
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 851HE
UT WOS:000297258200004
ER
PT J
AU Kliore, AJ
Nagy, AF
Cravens, TE
Richard, MS
Rymer, AM
AF Kliore, A. J.
Nagy, A. F.
Cravens, T. E.
Richard, M. S.
Rymer, A. M.
TI Unusual electron density profiles observed by Cassini radio occultations
in Titan's ionosphere: Effects of enhanced magnetospheric electron
precipitation?
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PLASMA
AB The Cassini radio science facility provided 13 occultation electron density profiles of Titan during the period of 2006 and 2009. This paper presents the results of all of these occultation observations. It shows that ten of the observed electron density profiles are similar, but three are significantly different. The number of observations is relatively small for meaningful statistical conclusions, but it is shown, using the corresponding measured electron spectra, that the three anomalous profiles in the ionospheric peak regions are likely to be the result of unusually intense electron precipitation events.
C1 [Kliore, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nagy, A. F.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Cravens, T. E.; Richard, M. S.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Rymer, A. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Kliore, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM akliore@jpl.nasa.gov
FU JPL; NASA-JPL [1416972, NAS5-97271, 1243218]; SWRI [NFP45280]; NASA
[NNX07AF46G]
FX The authors thank Don Mitchell for providing the electron flux data used
in Figure 4d. The work of A. J. Kliore was supported by the Cassini
program at JPL. The work of A. F. Nagy was supported by NASA-JPL
contract 1416972. The work of T. E. Cravens and M. S. Richard were
supported by the Cassini Program under SWRI sub-contract grant NFP45280
and NASA grant NNX07AF46G. Finally the work of A. M. Rymer was supported
by NASA-JPL contracts NAS5-97271 and 1243218.
NR 16
TC 12
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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 NOV 17
PY 2011
VL 116
AR A11318
DI 10.1029/2011JA016694
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 851HS
UT WOS:000297259600001
ER
PT J
AU Jacobson, NS
Myers, DL
AF Jacobson, Nathan S.
Myers, Dwight L.
TI High-Temperature Vaporization of B2O3(1) under Reducing Conditions
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID ELECTRON-IMPACT IONIZATION; MARK DM FORMALISM; CROSS-SECTIONS; BORIC
OXIDE; MOLECULAR STRUCTURE; MASS-SPECTROMETRY; SOLID ARGON; ATOMS;
BORON; SYSTEM
AB The vaporization of B2O3 in a reducing environment leads to the formation of both B2O3(g) and B2O2(g). Whereas the formation of B2O3(g) is well understood, many questions about the formation of B2O2(g) remain. Previous studies using B(s) + B2O3(1) have led to inconsistent thermodynamic data. In this study, it was found that, after heating, B(s) and B2O3(1) appeared to separate and variations in contact area likely led to the inconsistent vapor pressures of B2O2(g). To circumvent this problem, the activity of boron was fixed with a two-phase mixture of FeB and Fe2B. Both second- and third-law enthalpies of formation were measured for B2O2(g) and B2O3(g). From these values, the enthalpies of formation at 298.15 K were calculated to be -479.9 +/- 25.7 kJ/mol for B2O2(g) and -833.4 +/- 13.1 kJ/mol for B2O3(g). Ab initio calculations to determine the enthalpies of formation of B2O2(g) and B2O3(g) were conducted using the W1BD composite method and showed good agreement with the experimental values.
C1 [Jacobson, Nathan S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Myers, Dwight L.] E Cent Univ, Ada, OK 74820 USA.
RP Jacobson, NS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM nathan.s.jacobson@nasa.gov
NR 39
TC 6
Z9 6
U1 3
U2 10
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 NOV 17
PY 2011
VL 115
IS 45
BP 13253
EP 13260
DI 10.1021/jp206480d
PG 8
WC Chemistry, Physical
SC Chemistry
GA 843QB
UT WOS:000296686000015
PM 21957986
ER
PT J
AU Simoes, F
Pfaff, R
Freudenreich, H
AF Simoes, Fernando
Pfaff, Robert
Freudenreich, Henry
TI Satellite observations of Schumann resonances in the Earth's ionosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID PROPAGATION; ENVIRONMENT; CAVITY; TITAN
AB Using electric field measurements gathered on the C/NOFS satellite, we report, Schumann resonance signatures detected in space, well beyond the upper boundary of the resonant cavity formed by the earth's surface and the lower edge of the ionosphere. The resonances are routinely observed in the satellite ELF data during nighttime conditions within the altitude region of 400-850 km sampled by the satellite. They exhibit the distinctive frequency patterns predicted for Schumann resonances and are consistent with the corresponding frequency characteristics of ground-based observations of this phenomenon. The observations of Schumann resonances in space support a leaky cavity interpretation of the ionosphere and call for revisions of models of extremely low frequency wave propagation in the ionosphere. They suggest new remote sensing capabilities for investigating atmospheric electricity on Earth and other planets. Citation: Simoes, F., R. Pfaff, and H. Freudenreich (2011), Satellite observations of Schumann resonances in the Earth's ionosphere, Geophys. Res. Lett., 38, L22101, doi: 10.1029/2011GL049668.
C1 [Simoes, Fernando; Pfaff, Robert; Freudenreich, Henry] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Simoes, F (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 674,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM robert.f.pfaff@nasa.gov
RI Simoes, Fernando/D-7731-2012; Pfaff, Robert/F-5703-2012
OI Pfaff, Robert/0000-0002-4881-9715
FU USAF; Air Force Office of Scientific Research
FX The Communication/Navigation Outage Forecast System (C/NOFS) mission,
conceived and developed by the US Air Force Research Laboratory, is
sponsored and executed by the USAF Space Test Program. We acknowledge
support from the Air Force Office of Scientific Research. One of us (FS)
acknowledges the NASA Postdoctoral Program that is administered by the
Oak Ridge Associated Universities. We thank K. Bromund, C. Liebrecht,
and S. Martin for assistance with the data processing.
NR 24
TC 24
Z9 24
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD NOV 16
PY 2011
VL 38
AR L22101
DI 10.1029/2011GL049668
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 851HC
UT WOS:000297258000003
ER
PT J
AU Wang, L
Wolken, GJ
Sharp, MJ
Howell, SEL
Derksen, C
Brown, RD
Markus, T
Cole, J
AF Wang, L.
Wolken, G. J.
Sharp, M. J.
Howell, S. E. L.
Derksen, C.
Brown, R. D.
Markus, T.
Cole, J.
TI Integrated pan-Arctic melt onset detection from satellite active and
passive microwave measurements, 2000-2009
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SEA-ICE MELT; LAND-SURFACE SCHEME; SNOW-COVER; INTERANNUAL VARIABILITY;
CLIMATE MODELS; NORTH-AMERICA; MASS-BALANCE; CANADA; DURATION; ALBEDO
AB An integrated pan-Arctic melt onset data set is generated for the first time by combining estimates derived from active and passive microwave satellite data using algorithms developed for the northern high-latitude land surface, ice caps, large lakes, and sea ice. The data set yields new insights into the spatial and temporal patterns of mean melt onset date (MMOD) and the associated geographic and topographic controls. For example, in the terrestrial Arctic, tree fraction and latitude explain more than 60% of the variance in MMOD, with the former exerting a stronger influence on MMOD than the latter. Elevation is also found to be an important factor controlling MMOD, with most of the Arctic exhibiting significant positive relationships between MMOD and elevation, with a mean value of 24.5 m d(-1). Melt onset progresses fastest over land areas of uniform cover or elevation (40-80 km d(-1)) or both and slows down in mountainous areas, on ice caps, and in the forest-tundra ecotones. Over sea ice, melt onset advances very slowly in the marginal seas, while in the central Arctic the rate of advance can exceed 100 km d(-1). Comparison of the observed MMOD with simulated values from the third version of the Canadian Coupled Global Climate Model showed good agreement over land areas but weaker agreement over sea ice, particularly in the central Arctic, where simulated MMOD is about 2-3 weeks later than observed because of a cold bias in simulated surface air temperatures over sea ice.
C1 [Wang, L.; Howell, S. E. L.; Derksen, C.; Cole, J.] Environm Canada, Atmospher Sci & Technol Directorate, Div Climate Res, Toronto, ON M3H 5T4, Canada.
[Brown, R. D.] Ouranos Consortium Reg Climatol & Adaptat Climate, Montreal, PQ H3A 1B9, Canada.
[Markus, T.] NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wolken, G. J.] Alaska Div Geol & Geophys Surveys, Fairbanks, AK 99709 USA.
[Wolken, G. J.; Sharp, M. J.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
[Brown, R. D.] Environm Canada, Climate Res Div, Ouranos, Montreal, PQ, Canada.
RP Wang, L (reprint author), Environm Canada, Atmospher Sci & Technol Directorate, Div Climate Res, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada.
EM Libo.Wang@ec.gc.ca
RI Markus, Thorsten/D-5365-2012
FU Government of Canada Program for the International Polar Year
FX This study was carried out as part of the International Polar Year
project "Variability and Change in the Canadian Cryosphere," supported
by the Government of Canada Program for the International Polar Year.
The authors thank Warren Lee for providing the CGCM3 data, Mike Lazare
and Ed Chan for helpful discussion about CGCM3 outputs, Diana Verseghy
and Paul Bartlett for helpful discussion about snow simulations in
CLASS, and Yi Luo for providing MODIS clear-sky composite images. The
helpful comments from three anonymous referees are gratefully
acknowledged.
NR 74
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U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD NOV 16
PY 2011
VL 116
AR D22103
DI 10.1029/2011JD016256
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 851KI
UT WOS:000297267400005
ER
PT J
AU Boisson, J
Heggy, E
Clifford, SM
Yoshikawa, K
Anglade, A
Lognonne, P
AF Boisson, Josephine
Heggy, Essam
Clifford, Stephen M.
Yoshikawa, Kenji
Anglade, Andre
Lognonne, Philippe
TI Radar sounding of temperate permafrost in Alaska: Analogy to the Martian
midlatitude to high-latitude ice-rich terrains
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GROUND-PENETRATING RADAR; MEDUSAE FOSSAE FORMATION; LOBATE DEBRIS
APRONS; DIELECTRIC MEASUREMENTS; UTOPIA PLANITIA; CLIMATE-CHANGE;
SHALLOW RADAR; MARS; SUBSURFACE; WATER
AB Radar detection of subsurface ice on Mars has been widely debated in part because the dielectric signature of ice, as deduced from the dielectric constant, can be confused with dry-silicate-rich materials. To identify the ice dielectric signature, it is crucial to estimate the imaginary part of the dielectric permittivity inferred from the dielectric attenuation after removing the scattering loss. Unfortunately, the latter remains poorly quantified at both Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) and shallow subsurface radar SHARAD frequencies. To address this ambiguity, we conducted multiple-frequency ground-penetrating radar and resistivity investigations in well-characterized temperate permafrost in Fairbanks, Alaska. The area shows several geomorphologic similarities to midlatitude and high-latitude terrains on Mars. This approach allowed us to quantify the dielectric and scattering losses in temperate permafrost over the 10 to 1000 MHz frequency band. At 20 MHz, our results suggest an average dielectric loss rate of 0.25 +/- 0.03 dB/m, whereas the corresponding average scattering loss rate is 0.94 +/- 0.37 dB/m. The scattering loss was found to represent similar to 69% of the total signal attenuation. Considering this result and the study by Heggy et al. (2006a) in volcanic environments, we revised the interpretation of the attenuation coefficient calculated from SHARAD data over the Deuteronilus Mensae region and Amazonis Planitia; we then used the reevaluated dielectric loss to estimate the imaginary part of the dielectric permittivity. Our results suggest that even if Deuteronilus Mensae deposits and the Vastitas Borealis Formation may have similar dielectric constants, their imaginary parts are different. This implies that the two regions have different bulk compositions, with the former being ice-rich sediments and the latter being nonconsolidated volcanic deposits.
C1 [Boisson, Josephine; Anglade, Andre; Lognonne, Philippe] Inst Phys Globe Paris, F-94100 Saint Maur Des Fosses, France.
[Boisson, Josephine; Anglade, Andre; Lognonne, Philippe] Univ Paris Diderot, UMR CNRS 7154, Sorbonne Paris Cite, F-94100 Saint Maur Des Fosses, France.
[Clifford, Stephen M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Heggy, Essam] Jet Prop Lab, Pasadena, CA 91109 USA.
[Yoshikawa, Kenji] Univ Alaska Fairbanks, Water & Environm Res Ctr, Fairbanks, AK 99775 USA.
RP Boisson, J (reprint author), Inst Phys Globe Paris, 4 Ave Neptune, F-94100 Saint Maur Des Fosses, France.
EM boisson@ipgp.jussieu.fr; heggy@jpl.nasa.gov
RI Heggy, Essam/E-8250-2013; Lognonne, Philippe/F-8846-2010
OI Heggy, Essam/0000-0001-7476-2735;
FU NASA [NNG05GL39G, PGG04-000-0059]; Centre National d'Etudes Spatiales
(CNES); French Ministry of Research and Technology
FX We express our gratitude to Lucie Rolland and Fernand Lopes from IPGP
for the helpful discussions and comments. This work was supported in
part by NASA Mars Fundamental Research grant NNG05GL39G and by the NASA
Planetary Geology and Geophysics Program grant PGG04-000-0059.
Additional support was provided by Centre National d'Etudes Spatiales
(CNES) and by a French Ministry of Research and Technology Ph.D. grant
for Boisson. We are grateful to Steven A. Arcone and an anonymous
reviewer whose comments and suggestions were of great assistance in the
revision of the manuscript. 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. This is
IPGP contribution number 3212 and LPI contribution number 1561.
NR 101
TC 6
Z9 6
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD NOV 16
PY 2011
VL 116
AR E11003
DI 10.1029/2010JE003768
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 851KE
UT WOS:000297267000001
ER
PT J
AU Ott, L
Pawson, S
Bacmeister, J
AF Ott, Lesley
Pawson, Steven
Bacmeister, Julio
TI An analysis of the impact of convective parameter sensitivity on
simulated global atmospheric CO distributions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BIOMASS BURNING EMISSIONS; TROPOSPHERIC OZONE; TRACER TRANSPORT; MODEL;
CHEMISTRY; ENSEMBLE; PACIFIC; SYSTEM; ASIA
AB In an effort to better understand how uncertainty in simulated convection propagates into simulations of global trace gas distributions, we have constructed an eight-member ensemble of simulations using NASA's Goddard Earth Observing System Version 5 (GEOS-5) general circulation model (GCM). The ensemble was created by perturbing parameters in the model's moist physics schemes found to strongly influence the magnitude of convective mass flux. Globally, ensemble spreads in column CO are typically small (less than 4% of the mean column value) and, in many areas, are not significantly different from internal model variability. The largest ensemble spreads are found near source regions and outflow pathways. At the majority of remote surface monitoring sites, the annual mean ensemble spread is less than 5%, indicating that these locations, which are often the basis of inversion studies, are relatively insensitive to uncertainty in the representation of convection. We also examine in greater detail two simulations in which the magnitude of convective mass flux is significantly altered. Changes to convective parameters strongly influence grid-scale vertical and turbulent transport processes in addition to convective mass flux. Despite large differences in the magnitude of convective mass fluxes, this compensating behavior by other model processes results in comparable atmospheric residence times in the two simulations and largely similar global CO distributions. The results indicate that convective mass flux is strongly related to other vertical transport processes in a GCM and cannot be viewed as entirely separate. Future studies of the role of convective transport need to consider the relationship between convective and total mass flux.
C1 [Ott, Lesley; Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Ott, L (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-0, Greenbelt, MD 20771 USA.
EM lesley.e.ott@nasa.gov
RI Ott, Lesley/E-2250-2012; Pawson, Steven/I-1865-2014
OI Pawson, Steven/0000-0003-0200-717X
FU NASA
FX This research was funded by NASA's MAP program as part of a study to
understand the distribution and transport of carbon species in the
environment using GEOS-5. We thank Michele Rienecker for her support and
encouragement to perform this research in the GMAO. We are also grateful
to the three anonymous reviewers whose insightful comments greatly
enhanced this work.
NR 37
TC 13
Z9 13
U1 0
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 NOV 15
PY 2011
VL 116
AR D21310
DI 10.1029/2011JD016077
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 851KD
UT WOS:000297266900004
ER
PT J
AU Bosilovich, MG
Robertson, FR
Chen, JY
AF Bosilovich, Michael G.
Robertson, Franklin R.
Chen, Junye
TI Global Energy and Water Budgets in MERRA
SO JOURNAL OF CLIMATE
LA English
DT Article
ID 20TH-CENTURY CLIMATE VARIATIONS; LONG-TERM TRENDS; ANNUAL CYCLE;
SPATIOTEMPORAL STRUCTURE; REANALYSIS PROJECT; SURFACE-WATER; PART II;
PRECIPITATION; MODEL; LAND
AB Reanalyses, retrospectively analyzing observations over climatological time scales, represent a merger between satellite observations and models to provide globally continuous data and have improved over several generations. Balancing the earth's global water and energy budgets has been a focus of research for more than two decades. Models tend to their own climate while remotely sensed observations have had varying degrees of uncertainty. This study evaluates the latest NASA reanalysis, the Modern Era Retrospective-Analysis for Research and Applications (MERRA), from a global water and energy cycles perspective, to place it in context of previous work and demonstrate the strengths and weaknesses.
MERRA was configured to provide complete budgets in its output diagnostics, including the incremental analysis update (IAU), the term that represents the observations influence on the analyzed states, alongside the physical flux terms. Precipitation in reanalyses is typically sensitive to the observational analysis. For MERRA, the global mean precipitation bias and spatial variability are more comparable to merged satellite observations [the Global Precipitation and Climatology Project (GPCP) and Climate Prediction Center Merged Analysis of Precipitation (CMAP)] than previous generations of reanalyses. MERRA ocean evaporation also has a much lower value, which is comparable to independently derived estimate datasets. The global energy budget shows that MERRA cloud effects may be generally weak, leading to excess shortwave radiation reaching the ocean surface.
Evaluating the MERRA time series of budget terms, a significant change occurs that does not appear to be represented in observations. In 1999, the global analysis increments of water vapor changes sign from negative to positive and primarily lead to more oceanic precipitation. This change is coincident with the beginning of Advanced Microwave Sounding Unit (AMSU) radiance assimilation. Previous and current reanalyses all exhibit some sensitivity to perturbations in the observation record, and this remains a significant research topic for reanalysis development. The effect of the changing observing system is evaluated for MERRA water and energy budget terms.
C1 [Bosilovich, Michael G.; Chen, Junye] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Robertson, Franklin R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Chen, Junye] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
RP Bosilovich, MG (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM michael.bosilovich@nasa.gov
RI Bosilovich, Michael/F-8175-2012
FU NASA
FX MERRA was developed with support from the NASA Modeling, Analysis and
Prediction program. This study was supported by the NASA Energy and
Water cycles Studies (NEWS) program. The work also benefitted from
thoughtful comments from the NEWS Modeling working group and the NEWS
Global Energy Climatology working group. Siegfried Schubert, Kevin
Trenberth, and Paul Stackhouse also provided many thoughtful suggestions
over the course of this study. Russell Vose and Leopold Haimberger
provided valuable insights and discussions about the Bangui station. We
appreciate the useful comments and thoughtful review by four anonymous
reviewers.
NR 50
TC 108
Z9 109
U1 3
U2 39
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD NOV 15
PY 2011
VL 24
IS 22
BP 5721
EP 5739
DI 10.1175/2011JCLI4175.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 849PX
UT WOS:000297138700001
ER
PT J
AU Svensson, G
Karlsson, J
AF Svensson, Gunilla
Karlsson, Johannes
TI On the Arctic Wintertime Climate in Global Climate Models
SO JOURNAL OF CLIMATE
LA English
DT Article
ID POLAR PATHFINDER DATASET; SURFACE-ENERGY BUDGET; RADIATION PROPERTIES;
VERTICAL STRUCTURE; ERA-40 REANALYSIS; COUPLED MODELS; BOUNDARY-LAYER;
RECENT TRENDS; CLOUD; SIMULATIONS
AB Energy fluxes important for determining the Arctic surface temperatures during winter in present-day simulations from the Coupled Model lntercomparison Project phase 3 (CMIP3) multimodel dataset are investigated. The model results are evaluated over different surfaces using satellite retrievals and ECMWF interim reanalysis (ERA-Interim). The wintertime turbulent heat fluxes vary substantially between models and different surfaces. The monthly median net turbulent heat flux (upward) is in the range 100-200 W m(-2) and 15 to 15 W m(-2) over open ocean and sea ice, respectively. The simulated net longwave radiative flux at the surface is biased high over both surfaces compared to observations but for different reasons. Over open ocean, most models overestimate the outgoing longwave flux while over sea ice it is rather the downwelling flux that is underestimated. Based on the downwelling longwave flux over sea ice, two categories of models are found. One group of models that shows reasonable downwelling longwave fluxes, compared with observations and ERA-Interim, is also associated with relatively high amounts of precipitable water as well as surface skin temperatures. This group also shows more uniform airmass properties over the Arctic region possibly as a result of more frequent events of warm-air intrusion from lower latitudes. The second group of models underestimates the downwelling longwave radiation and is associated with relatively low surface skin temperatures as well as low amounts of precipitable water. These models also exhibit a larger decrease in the moisture and temperature profiles northward in the Arctic region, which might be indicative of too stagnant conditions in these models.
C1 [Svensson, Gunilla] Stockholm Univ, Dept Meteorol, SE-10691 Stockholm, Sweden.
[Karlsson, Johannes] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Svensson, G (reprint author), Stockholm Univ, Dept Meteorol, SE-10691 Stockholm, Sweden.
EM gunilla@misu.su.se
RI Karlsson, Johannes/H-3937-2011
NR 40
TC 17
Z9 17
U1 1
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD NOV 15
PY 2011
VL 24
IS 22
BP 5757
EP 5771
DI 10.1175/2011JCLI4012.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 849PX
UT WOS:000297138700003
ER
PT J
AU Mishchenko, MI
Dlugach, JM
Mackowski, DW
AF Mishchenko, Michael I.
Dlugach, Janna M.
Mackowski, Daniel W.
TI Coherent backscattering by polydisperse discrete random media: exact
T-matrix results
SO OPTICS LETTERS
LA English
DT Article
ID SCATTERING; ABSORPTION; PARTICLES; LIGHT
AB The numerically exact superposition T-matrix method is used to compute, for the first time to our knowledge, electromagnetic scattering by finite spherical volumes composed of polydisperse mixtures of spherical particles with different size parameters or different refractive indices. The backscattering patterns calculated in the far-field zone of the polydisperse multiparticle volumes reveal unequivocally the classical manifestations of the effect of weak localization of electromagnetic waves in discrete random media, thereby corroborating the universal interference nature of coherent backscattering. The polarization opposition effect is shown to be the least robust manifestation of weak localization fading away with increasing particle size parameter. (C) 2011 Optical Society of America
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
RI Mackowski, Daniel/K-1917-2013; Mishchenko, Michael/D-4426-2012
FU Ukrainian National Academy of Sciences; National Aeronautics and Space
Administration (NASA)
FX We are grateful to Karri Muinonen, Vera Rosenbush, and Victor Tishkovets
for many useful discussions. We acknowledge support from the Ukrainian
National Academy of Sciences under the Main Astronomical Observatory
GRAPE/CPU/GRID computer cluster project. This research was supported by
the National Aeronautics and Space Administration (NASA) Radiation
Sciences Program managed by Hal Maring.
NR 18
TC 2
Z9 3
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 NOV 15
PY 2011
VL 36
IS 22
BP 4350
EP 4352
PG 3
WC Optics
SC Optics
GA 850RL
UT WOS:000297215300014
PM 22089560
ER
PT J
AU Xu, F
Davis, AB
AF Xu, Feng
Davis, Anthony B.
TI Derivatives of light scattering properties of a nonspherical particle
computed with the T-matrix method
SO OPTICS LETTERS
LA English
DT Article
AB Based on the T-matrix formalism, we analytically calculate derivatives of light scattering quantities by a nonspherical particle with respect to its microphysical parameters. Illustrative computations are performed for a spheroid, and the results agree with those obtained by finite differencing. The proposed formalism also predicts correctly derivatives for a sphere obtained by linearized Lorenz-Mie theory. (C) 2011 Optical Society of America
C1 [Xu, Feng; Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Xu, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Feng.Xu@jpl.nasa.gov
RI Xu, Feng/G-3673-2013
FU National Aeronautics and Space Administration (NASA), U.S. government
FX This work was done at the Jet Propulsion Laboratory, California
Institute of Technology under contract with the National Aeronautics and
Space Administration (NASA), U.S. government sponsorship acknowledged.
NR 12
TC 4
Z9 5
U1 0
U2 3
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 NOV 15
PY 2011
VL 36
IS 22
BP 4464
EP 4466
PG 3
WC Optics
SC Optics
GA 850RL
UT WOS:000297215300052
PM 22089598
ER
PT J
AU Mawhorter, RJ
Greenwood, JB
Chutjian, A
Haley, T
Mitescu, CD
Simcic, J
AF Mawhorter, R. J.
Greenwood, J. B.
Chutjian, A.
Haley, T.
Mitescu, C. D.
Simcic, J.
TI Measurement of absolute charge-exchange cross sections for He2+
collisions with He and H-2
SO PHYSICAL REVIEW A
LA English
DT Article
ID DOUBLE-ELECTRON CAPTURE; X-RAY-EMISSION; SINGLE-ELECTRON; SOLAR-WIND;
HE-2+-HE COLLISIONS; ENERGY-RANGE; SLOW HE2+; IONS; SCATTERING; SYSTEM
AB Reported are total, absolute charge-exchange cross sections for collisions of 3He(2+) ions with He and H-2. Measurements are reported at fixed energies between 0.33 and 4.67 keV/amu. Both the present results and earlier results of others are analyzed in terms of available experimental small-angle differential cross sections as a function of collision energy, and hence the geometry of the exit aperture of the gas-collision cells used by the various experimental groups. In addition, the effective length of gas-collision cells is studied using fluid dynamic and molecular flow simulations to address the density patterns near the cell entrance and exit apertures. When small acceptance-angle corrections were applied, the results of present and previous measurements for the single electron capture in these systems were brought into good accord in the relevant energy ranges. Taken in their entirety, the present data for 3He(2+) with He and H-2 lend themselves to new theoretical calculations of the multichannel charge-exchange cross sections.
C1 [Mawhorter, R. J.; Chutjian, A.; Simcic, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mawhorter, R. J.; Haley, T.; Mitescu, C. D.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Greenwood, J. B.] Queens Univ Belfast, Dept Phys, Belfast BT7 1NN, Antrim, North Ireland.
RP Mawhorter, RJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Greenwood, Jason/L-4799-2014
FU National Aeronautics and Space Administration
FX We thank C. R. Vane for informative discussions and for carrying out the
alternative gas-cell effective-length calculation, and D.
Bordenave-Montesquieu for providing differential cross sections in
tabular form. We also thank L. Mendez for helpful discussions on the
theory. This work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology and was supported through an
agreement with the National Aeronautics and Space Administration.
NR 57
TC 6
Z9 6
U1 0
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD NOV 15
PY 2011
VL 84
IS 5
AR 052714
DI 10.1103/PhysRevA.84.052714
PG 8
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 849AA
UT WOS:000297095100007
ER
PT J
AU Mora, MF
Greer, F
Stockton, AM
Bryant, S
Willis, PA
AF Mora, Maria F.
Greer, Frank
Stockton, Amanda M.
Bryant, Sherrisse
Willis, Peter A.
TI Toward Total Automation of Microfluidics for Extraterrestial In Situ
Analysis
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID MICROCHIP-CAPILLARY-ELECTROPHORESIS; IONIZATION-MASS SPECTROMETRY;
FUSED-SILICA CAPILLARIES; MARS ORGANIC ANALYZER; AMINO-ACIDS; MEMBRANE
VALVES; PUMPS; BIOMARKERS; CHIP; INSTRUMENTATION
AB Despite multiple orbiter and landed missions to extraterrestrial bodies in the solar system, including Mars and Titan, we still know relatively little about the detailed chemical composition and quantity of organics and biomolecules in those bodies. For chemical analysis on astrobiologically relevant targets such as Mars, Europa, Titan, and Enceladus, instrumentation should be extremely sensitive and capable of analyzing a broad range of organic molecules. Microchip capillary electrophoresis (mu CE) with laser-induced fluorescence (LIF) detection provides this required sensitivity and targets a wide range of relevant markers but, to date, has lacked the necessary degree of automation for spaceflight applications. Here we describe a fully integrated microfluidic device capable of performing automated end-to-end analyses of amino acids by mu CE with LIF detection. The device integrates an array of pneumatically actuated valves and pumps for autonomous fluidic routing with an electrophoretic channel. Operation of the device, including manipulation of liquids for sample pretreatment and electrophoretic analysis, was performed exclusively via computer control. The device was validated by mixing of laboratory standards and labeling of amino acids with Pacific Blue succinimidyl ester followed by electrophoretic analysis. To our knowledge, this is the first demonstration of completely automated end-to-end mu CE analyses on a single, fully integrated microfluidic device.
C1 [Mora, Maria F.; Greer, Frank; Stockton, Amanda M.; Bryant, Sherrisse; Willis, Peter A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Willis, PA (reprint author), CALTECH, Jet Prop Lab, Mail Stop 302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM peter.a.willis@jpl.nasa.gov
RI Stockton, Amanda/C-1173-2012; Mora, Maria/C-9753-2009; Willis,
Peter/I-6621-2012
FU NASA [104320]; NASA at the Jet Propulsion Laboratory
FX The first two authors contributed equally to this work. 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. Financial support for
this project was provided by NASA's Astrobiology Science and Technology
Instrument Development (ASTID) Program (Project #104320), the NASA
Harriett G. Jenkins Predoctoral Fellowship Project (JPFP) Mini Research
Award, and the NASA Postdoctoral Program (NPP) at the Jet Propulsion
Laboratory, administered by Oak Ridge Associated Universities through a
contract with NASA. We thank Dr. Morgan L. Cable for her help with the
fluorescence measurements, and Dr. Adrian Ponce's lab for the use of the
Fluorolog-3 fluorescence spectrometer.
NR 37
TC 26
Z9 26
U1 5
U2 43
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
J9 ANAL CHEM
JI Anal. Chem.
PD NOV 15
PY 2011
VL 83
IS 22
BP 8636
EP 8641
DI 10.1021/ac202095k
PG 6
WC Chemistry, Analytical
SC Chemistry
GA 845NQ
UT WOS:000296830200040
PM 21972965
ER
PT J
AU Shay, JW
Cucinotta, FA
Sulzman, FM
Coleman, CN
Minna, JD
AF Shay, Jerry W.
Cucinotta, Francis A.
Sulzman, Frank M.
Coleman, C. Norman
Minna, John D.
TI From Mice and Men to Earth and Space: Joint NASA-NCI Workshop on Lung
Cancer Risk Resulting from Space and Terrestrial Radiation
SO CANCER RESEARCH
LA English
DT Editorial Material
AB On June 27-28, 2011, scientists from the National Cancer Institute (NCI), NASA, and academia met in Bethesda to discuss major lung cancer issues confronting each organization. For NASA, available data suggest that lung cancer is the largest potential cancer risk from space travel for both men and women and quantitative risk assessment information for mission planning is needed. In space, the radiation risk is from high energy and charge (HZE) nuclei (such as Fe) and high-energy protons from solar flares and not from gamma radiation. In contrast, the NCI is endeavoring to estimate the increased lung cancer risk from the potential widespread implementation of computed tomographic (CT) screening in individuals at high risk for developing lung cancer based on the National Lung Cancer Screening Trial (NLST). For the latter, exposure will be X-rays from CT scans from the screening (which uses "low-dose" CT scans) and also from follow-up scans used to evaluate abnormalities found during initial screening. Topics discussed included the risk of lung cancer arising after HZE particle, proton, and low-dose exposure to Earth's radiation. The workshop examined preclinical models, epidemiology, molecular markers, "omics" technology, radiobiology issues, and lung stem cells that relate to the development of lung cancer. Cancer Res; 71(22); 6926-9. (C)2011 AACR.
C1 [Shay, Jerry W.; Minna, John D.] Univ Texas SW Med Ctr Dallas, Dallas, TX 75390 USA.
[Cucinotta, Francis A.; Sulzman, Frank M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Coleman, C. Norman] NCI, Radiat Res Program, Bethesda, MD 20892 USA.
RP Shay, JW (reprint author), Univ Texas SW Med Ctr Dallas, Dallas, TX 75390 USA.
EM Jerry.Shay@utsouthwestern.edu
FU NCI NIH HHS [P50 CA070907, T32 CA124334, P50 CA070907-10, T32
CA124334-05]
NR 0
TC 9
Z9 9
U1 0
U2 6
PU AMER ASSOC CANCER RESEARCH
PI PHILADELPHIA
PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA
SN 0008-5472
J9 CANCER RES
JI Cancer Res.
PD NOV 15
PY 2011
VL 71
IS 22
BP 6926
EP 6929
DI 10.1158/0008-5472.CAN-11-2546
PG 4
WC Oncology
SC Oncology
GA 847NS
UT WOS:000296980200003
PM 21900398
ER
PT J
AU Joy, KH
Kring, DA
Bogard, DD
McKay, DS
Zolensky, ME
AF Joy, Katherine H.
Kring, David A.
Bogard, Donald D.
McKay, David S.
Zolensky, Michael E.
TI Re-examination of the formation ages of the Apollo 16 regolith breccias
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID INNER SOLAR-SYSTEM; LATE HEAVY BOMBARDMENT; IMPACT MELT ROCKS; NOBLE-GAS
ISOTOPES; LUNAR CATACLYSM; CENTRAL-HIGHLANDS; ASTEROID BELT; LANDING
SITES; RAY CRATER; MOON
AB The lunar regolith is exposed to irradiation from the solar wind and to bombardment by asteroids, comets and inter-planetary dust. Fragments of projectiles in the lunar regolith can potentially provide a direct measure of the sources of exogenous material being delivered to the Moon. Constraining the temporal flux of their delivery helps to address key questions about the bombardment history of the inner Solar System.
Here, we use a revised antiquity calibration (after Eugster et al., 2001) that utilises the ratio of trapped Ar-40/Ar-36 ('parentless' Ar-40 derived from radioactive decay of K-40, against solar wind derived Ar-36) to semi-quantitatively calculate the timing of the assembly of the Apollo 16 regolith breccias. We use the trapped Ar-40/Ar-36 ratios reported by McKay et al. (1986). Our model indicates that the Apollo 16 ancient regolith breccia population was formed between similar to 3.8 and 3.4 Ga, consistent with regoliths developed and assembled after the Imbrium basin-forming event at similar to 3.85 Ga, and during a time of declining basin-forming impacts. The material contained within the ancient samples potentially provides evidence of impactors delivered to the Moon in the Late-Imbrian epoch. We also find that a young regolith population was assembled, probably by local impacts in the Apollo 16 area, in the Eratosthenian period between similar to 2.5 and 2.2 Ga, providing insights to the sources of post-basin bombardment. The 'soil-like' regolith breccia population, and the majority of local Apollo 16 soils, were likely closed in the last 2 Ga and, therefore, potentially provide an archive of projectile types in the Eratosthenian and Copernican periods. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Joy, Katherine H.; Kring, David A.; Bogard, Donald D.] Lunar & Planetary Inst USRA, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA.
[Joy, Katherine H.; Kring, David A.; Bogard, Donald D.; McKay, David S.; Zolensky, Michael E.] NASA, Lunar Sci Inst, Washington, DC USA.
[Bogard, Donald D.; McKay, David S.; Zolensky, Michael E.] NASA, Johnson Space Ctr, ARES, Washington, DC USA.
RP Joy, KH (reprint author), Lunar & Planetary Inst USRA, Ctr Lunar Sci & Explorat, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM joy@lpi.usra.edu
OI Joy, Katherine/0000-0003-4992-8750
FU NASA Lunar Science Institute [NNA09D-B33A]
FX We would like to thank Drs. Vera Fernandes and Marc Norman for careful
reviews of this manuscript, and to Dr. Christian Koeberl for editorial
guidance. Thanks also to Dr. Paul Spudis for discussions about the
geological history of the Apollo 16 landing site and to Dr. Marion
Grange for advice regarding recalibration of Ar-Ar isotope age dates.
Katherine H. Joy is an honorary research associate of the UCL Dept. of
Earth Sciences and would like to thank UCL for access to electronic
resources. This research was funded by NASA Lunar Science Institute
contract NNA09D-B33A David A. Kring PI. This is LPI contribution number
1637.
NR 133
TC 17
Z9 17
U1 1
U2 10
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 NOV 15
PY 2011
VL 75
IS 22
BP 7208
EP 7225
DI 10.1016/j.gca.2011.09.018
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 842FQ
UT WOS:000296579600029
ER
PT J
AU Allen, MS
Hertz, PL
AF Allen, Marc S.
Hertz, Paul L.
TI Starting to partner with NASA in space and Earth science
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Partnering with NASA; Space science; Earth science; Ground-based
measurements; Suborbital investigations; GLOBE program
AB NASA research programs offer many opportunities for productive partnerships with investigators in other countries. While spacecraft projects are complex and very expensive, there are other, lower-cost partnerships that can yield important scientific results and offer excellent opportunities for building up new space and Earth science programs and for training new researchers. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Allen, Marc S.; Hertz, Paul L.] NASA, Sci Mission Directorate, Washington, DC 20546 USA.
RP Allen, MS (reprint author), NASA, Sci Mission Directorate, 300 E St SW, Washington, DC 20546 USA.
EM marc.allen@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 2
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD NOV 15
PY 2011
VL 48
IS 10
BP 1638
EP 1642
DI 10.1016/j.asr.2011.08.013
PG 5
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 834WC
UT WOS:000295994200010
ER
PT J
AU Mason, J
Stupl, J
Marshall, W
Levit, C
AF Mason, James
Stupl, Jan
Marshall, William
Levit, Creon
TI Orbital debris-debris collision avoidance
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Space debris; Collision avoidance; Conjunction analysis; Kessler
syndrome; Active debris removal; Laser
ID LASER; LEO; SYSTEM; BEAM
AB We focus on preventing collisions between debris and debris, for which there is no current, effective mitigation strategy. We investigate the feasibility of using a medium-powered (5 kW) ground-based laser combined with a ground-based telescope to prevent collisions between debris objects in low-Earth orbit (LEO). The scheme utilizes photon pressure alone as a means to perturb the orbit of a debris object. Applied over multiple engagements, this alters the debris orbit sufficiently to reduce the risk of an upcoming conjunction. We employ standard assumptions for atmospheric conditions and the resulting beam propagation. Using case studies designed to represent the properties (e.g. area and mass) of the current debris population, we show that one could significantly reduce the risk of nearly half of all catastrophic collisions involving debris using only one such laser/telescope facility. We speculate on whether this could mitigate the debris fragmentation rate such that it falls below the natural debris re-entry rate due to atmospheric drag, and thus whether continuous long-term operation could entirely mitigate the Kessler syndrome in LEO, without need for relatively expensive active debris removal. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Mason, James; Marshall, William; Levit, Creon] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Mason, James; Marshall, William] Univ Space Res Assoc, Moffett Field, CA 94035 USA.
[Stupl, Jan] Stanford Univ, Ctr Int Secur & Cooperat, Stanford, CA 94305 USA.
RP Mason, J (reprint author), NASA, Ames Res Ctr, MS202-3, Moffett Field, CA 94035 USA.
EM james.mason@nasa.gov
NR 37
TC 23
Z9 23
U1 0
U2 19
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 NOV 15
PY 2011
VL 48
IS 10
BP 1643
EP 1655
DI 10.1016/j.asr.2011.08.005
PG 13
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 834WC
UT WOS:000295994200011
ER
PT J
AU Mondal, SP
Dutta, PK
Hunter, GW
Ward, BJ
Laskowski, D
Dweik, RA
AF Mondal, Suvra Prakash
Dutta, Prabir K.
Hunter, G. W.
Ward, B. J.
Laskowski, D.
Dweik, R. A.
TI Development of high sensitivity potentiometric NOx sensor and its
application to breath analysis
SO SENSORS AND ACTUATORS B-CHEMICAL
LA English
DT Article
DE Harsh environment sensor; Combustion sensor; Biomarkers of disease;
Asthma monitoring; Interferences
ID QUANTUM-CASCADE LASER; NITRIC-OXIDE; GAS SENSOR; SPECTROSCOPIC
DETECTION; TEMPERATURE; FABRICATION; ELECTRODES; DISEASES; FILTER;
OXYGEN
AB Using a combination of similar potentiometric sensors connected in series, a strategy for measuring NO at ppb concentrations has been demonstrated. Sensors numbering from 2 to 20 were fabricated, with each sensor based on YSZ electrolyte with WO3 sensing electrode and Pt-zeolite/Pt as the reference electrode. Use of a catalytic filter allows for the cancellation of interferences due to oxidizable gases, such as CO. The optimum operating temperature of the filter and sensor was determined to be 250 and 425 degrees C, respectively. For human breath samples, the interference from water was acute enough that only scrubbing through a dry ice/acetone bath led to adequate performance for detection of NO in the 5-80 ppb range with a 20-sensor array. A more practical strategy suitable for clinical analysis was demonstrated by using water saturated air as the background gas. A linear calibration curve in the range suitable for use in clinical analysis is demonstrated. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Mondal, Suvra Prakash; Dutta, Prabir K.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA.
[Hunter, G. W.] NASA, Glenn Res Ctr, Sensors & Elect Branch, Chem Species Gas Sensors Team, Cleveland, OH USA.
[Ward, B. J.] Makel Engn Inc, Chico, CA USA.
[Laskowski, D.; Dweik, R. A.] Cleveland Clin Fdn, Cleveland, OH 44195 USA.
RP Dutta, PK (reprint author), Ohio State Univ, Dept Chem, Columbus, OH 43210 USA.
EM dutta.1@osu.edu
FU state of Ohio
FX We acknowledge funding from the Third Frontier grant from the state of
Ohio.
NR 32
TC 27
Z9 28
U1 5
U2 52
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-4005
J9 SENSOR ACTUAT B-CHEM
JI Sens. Actuator B-Chem.
PD NOV 15
PY 2011
VL 158
IS 1
BP 292
EP 298
DI 10.1016/j.snb.2011.05.063
PG 7
WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation
SC Chemistry; Electrochemistry; Instruments & Instrumentation
GA 828KP
UT WOS:000295500200041
ER
PT J
AU West, WC
Staniewicz, RJ
Ma, C
Robak, J
Soler, J
Smart, MC
Ratnakumar, BV
AF West, W. C.
Staniewicz, R. J.
Ma, C.
Robak, J.
Soler, J.
Smart, M. C.
Ratnakumar, B. V.
TI Implications of the first cycle irreversible capacity on cell balancing
for Li2MnO3-LiMO2 (M = Ni, Mn, Co) Li-ion cathodes
SO JOURNAL OF POWER SOURCES
LA English
DT Article
DE Irreversible capacity; MoS2; Li-ion; Cathode; Cell balancing
ID OXYGEN LOSS; LITHIUM; BATTERIES; ELECTRODES
AB Much of the research on lithium-ion cathodes consisting of layered solid solutions of Li2MnO3-LiMO2 (M = Mn, Co, Ni) has focused on identifying the causes of the irreversible capacity loss on the first cycle. However, a key issue that must be addressed is whether the high irreversible capacity observed seen on the first cycle is associated with intercalated lithium at the anode, or if it is associated with irretrievable capacity (i.e., film formation, and/or decomposition reactions). To this end, we have quantified the amount of utilizable lithium that is made available for the anodes when employing Li2MnO3-LiMO2 as cathodes. Using a MoS2 anode lithiation plateau transition as a reference point to the amount of lithium transferred to the anode during charge, it has been shown that almost none of the cathode irreversible charge capacity resulted in lithiation of the anode. Further, by reacting charged graphitic anodes that were retrieved from C anode-Li1.2Ni0.175Co0.1Mn0.52O2 cathode cells with water to generate H-2 gas to measure the active amount of lithium in the anode, we confirmed the results with the MoS2 titration experiments, demonstrating that lithium released from the cathode during the first charge is not proportionate to the cathode charge capacity. (C) 2011 Elsevier B.V. All rights reserved.
C1 [West, W. C.; Soler, J.; Smart, M. C.; Ratnakumar, B. V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Staniewicz, R. J.; Ma, C.; Robak, J.] Soft America Inc, Space & Def Div US, Cockeysville, MD 21030 USA.
RP West, WC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM william.c.west@jpl.nasa.gov
FU NASA
FX This work was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. The authors wish to thank James
Kulleck for carrying out the X-ray diffraction measurements. The authors
acknowledge the funding support of NASA's Exploration Technology
Development Program.
NR 15
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-7753
J9 J POWER SOURCES
JI J. Power Sources
PD NOV 15
PY 2011
VL 196
IS 22
BP 9696
EP 9701
DI 10.1016/j.jpowsour.2011.07.050
PG 6
WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials
Science, Multidisciplinary
SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science
GA 829RQ
UT WOS:000295602400079
ER
PT J
AU Hall, F
Saatchi, S
Dubayah, R
AF Hall, Forrest
Saatchi, Sassan
Dubayah, Ralph
TI PREFACE: DESDynI VEG-3D Special Issue
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Editorial Material
C1 [Saatchi, Sassan] NASA, Jet Prop Lab, Washington, DC 20546 USA.
[Dubayah, Ralph] Univ Maryland, College Pk, MD 20742 USA.
RP Saatchi, S (reprint author), NASA, Jet Prop Lab, Washington, DC 20546 USA.
EM sasan.s.saatchi@jpl.nasa.gov
NR 0
TC 5
Z9 5
U1 0
U2 6
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 NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2752
EP 2752
DI 10.1016/j.rse.2011.04.014
PG 1
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400002
ER
PT J
AU Hall, FG
Bergen, K
Blair, JB
Dubayah, R
Houghton, R
Hurtt, G
Kellndorfer, J
Lefsky, M
Ranson, J
Saatchi, S
Shugart, HH
Wickland, D
AF Hall, Forrest G.
Bergen, Kathleen
Blair, James B.
Dubayah, Ralph
Houghton, Richard
Hurtt, George
Kellndorfer, Josef
Lefsky, Michael
Ranson, Jon
Saatchi, Sasan
Shugart, H. H.
Wickland, Diane
TI Characterizing 3D vegetation structure from space: Mission requirements
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Biomass; 3D vegetation tructure; Carbon cycle; Remote sensing; Radar;
Lidar; DESDynI
ID BAND RADAR BACKSCATTER; POLARIMETRIC SAR INTERFEROMETRY; MAPPING FOREST
STRUCTURE; LARGE-FOOTPRINT LIDAR; SIR-C/X-SAR; TROPICAL FOREST;
ABOVEGROUND BIOMASS; AIRBORNE LIDAR; BOREAL FOREST; SPECIES-DIVERSITY
AB Human and natural forces are rapidly modifying the global distribution and structure of terrestrial ecosystems on which all of life depends, altering the global carbon cycle, affecting our climate now and for the foreseeable future, causing steep reductions in species diversity, and endangering Earth's sustainability.
To understand changes and trends in terrestrial ecosystems and their functioning as carbon sources and sinks, and to characterize the impact of their changes on climate, habitat and biodiversity, new space assets are urgently needed to produce high spatial resolution global maps of the three-dimensional (3D) structure of vegetation, its biomass above ground, the carbon stored within and the implications for atmospheric green house gas concentrations and climate. These needs were articulated in a 2007 National Research Council (NRC) report (NRC, 2007) recommending a new satellite mission, DESDynI, carrying an L-band Polarized Synthetic Aperture Radar (Pol-SAR) and a multi-beam lidar (light RAnging And Detection) operating at 1064 nm. The objectives of this paper are to articulate the importance of these new, multi-year, 3D vegetation structure and biomass measurements, to briefly review the feasibility of radar and lidar remote sensing technology to meet these requirements, to define the data products and measurement requirements, and to consider implications of mission durations. The paper addresses these objectives by synthesizing research results and other input from a broad community of terrestrial ecology, carbon cycle, and remote sensing scientists and working groups. We conclude that:
(1) Current global biomass and 3-D vegetation structure information is unsuitable for both science and management and policy. The only existing global datasets of biomass are approximations based on combining land cover type and representative carbon values, instead of measurements of actual biomass. Current measurement attempts based on radar and multispectral data have low explanatory power outside low biomass areas. There is no current capability for repeatable disturbance and regrowth estimates.
(2) The science and policy needs for information on vegetation 3D structure can be successfully addressed by a mission capable of producing (i) a first global inventory of forest biomass with a spatial resolution 1 km or finer and unprecedented accuracy (ii) annual global disturbance maps at a spatial resolution of 1 ha with subsequent biomass accumulation rates at resolutions of 1 km or finer, and (iii) transects of vertical and horizontal forest structure with 30 m along-transect measurements globally at 25 m spatial resolution, essential for habitat characterization.
We also show from the literature that lidar profile samples together with wall-to-wall L-band quad-pol-SAR imagery and ecosystem dynamics models can work together to satisfy these vegetation 3D structure and biomass measurement requirements. Finally we argue that the technology readiness levels of combined pol-SAR and lidar instruments are adequate for space flight. Remaining to be worked out, are the particulars of a lidar/pol-SAR mission design that is feasible and at a minimum satisfies the information and measurement requirement articulated herein. (C) 2011 Published by Elsevier Inc.
C1 [Hall, Forrest G.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Bergen, Kathleen] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA.
[Blair, James B.; Ranson, Jon] NASA, Goddard Space Flight Ctr, Washington, DC USA.
[Dubayah, Ralph] Univ Maryland, Univ Coll, Dept Geog, College Pk, MD 20742 USA.
[Wickland, Diane] NASA Headquarters, Washington, DC USA.
[Houghton, Richard; Kellndorfer, Josef] Woods Hole Res Ctr, Woods Hole, MA USA.
[Hurtt, George] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Shugart, H. H.] Univ Virginia, Dept Environm Sci, Charlottesville, VA USA.
[Lefsky, Michael] Colorado State Univ, Dept Forestry, Ft Collins, CO 80523 USA.
RP Hall, FG (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
EM Forrest.G.Hall@nasa.gov
RI Hurtt, George/A-8450-2012; Blair, James/D-3881-2013; chen,
zhu/K-5923-2013; Shugart, Herman/C-5156-2009
NR 165
TC 87
Z9 95
U1 12
U2 99
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 NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2753
EP 2775
DI 10.1016/j.rse.2011.01.024
PG 23
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400003
ER
PT J
AU Pang, Y
Lefsky, M
Sun, GQ
Ranson, J
AF Pang, Yong
Lefsky, Michael
Sun, Guoqing
Ranson, Jon
TI Impact of footprint diameter and off-nadir pointing on the precision of
canopy height estimates from spaceborne lidar
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Spaceborne lidar; Lidar waveform simulation; Off-nadir pointing;
Footprint diameter; Canopy height; DESDynI; ICESat-II
ID WAVE-FORMS; FOREST; REFLECTANCE
AB A spaceborne lidar mission could serve multiple scientific purposes including remote sensing of ecosystem structure, carbon storage, terrestrial topography and ice sheet monitoring. The measurement requirements of these different goals will require compromises in sensor design. Footprint diameters that would be larger than optimal for vegetation studies have been proposed. Some spaceborne lidar mission designs include the possibility that a lidar sensor would share a platform with another sensor, which might require off-nadir pointing at angles of up to 16 degrees. To resolve multiple mission goals and sensor requirements, detailed knowledge of the sensitivity of sensor performance to these aspects of mission design is required.
This research used a radiative transfer model to investigate the sensitivity of forest height estimates to footprint diameter, off-nadir pointing and their interaction over a range of forest canopy properties. An individual-based forest model was used to simulate stands of mixed conifer forest in the Tahoe National Forest (Northern California, USA) and stands of deciduous forests in the Bartlett Experimental Forest (New Hampshire, USA). Waveforms were simulated for stands generated by a forest succession model using footprint diameters of 20 m to 70 m. Off-nadir angles of 0 to 16 degrees were considered for a 25 m diameter footprint diameter.
Footprint diameters in the range of 25 m to 30 m were optimal for estimates of maximum forest height (R-2 of 0.95 and RMSE of 3 m). As expected, the contribution of vegetation height to the vertical extent of the waveform decreased with larger footprints, while the contribution of terrain slope increased. Precision of estimates decreased with an increasing off-nadir pointing angle, but off-nadir pointing had less impact on height estimates in deciduous forests than in coniferous forests. When pointing off-nadir, the decrease in precision was dependent on local incidence angle (the angle between the off-nadir beam and a line normal to the terrain surface)which is dependent on the off-nadir pointing angle, terrain slope, and the difference between the laser pointing azimuth and terrain aspect; the effect was larger when the sensor was aligned with the terrain azimuth but when aspect and azimuth are opposed, there was virtually no effect on R-2 or RMSE. A second effect of off-nadir pointing is that the laser beam will intersect individual crowns and the canopy as a whole from a different angle which had a distinct effect on the precision of lidar estimates of height, decreasing R-2 and increasing RMSE, although the effect was most pronounced for coniferous crowns. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Pang, Yong; Lefsky, Michael] Colorado State Univ, Ctr Ecol Applicat Lidar, Warner Coll Nat Resources, Ft Collins, CO 80523 USA.
[Pang, Yong] Chinese Acad Forestry, Inst Forest Resource Informat Tech, Beijing 100091, Peoples R China.
[Sun, Guoqing] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Ranson, Jon] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lefsky, M (reprint author), Colorado State Univ, Ctr Ecol Applicat Lidar, Warner Coll Nat Resources, Ft Collins, CO 80523 USA.
EM lefsky@cnr.colostate.edu
RI Pang, Yong/J-2218-2012
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2798
EP 2809
DI 10.1016/j.rse.2010.08.025
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400006
ER
PT J
AU Saatchi, S
Marlier, M
Chazdon, RL
Clark, DB
Russell, AE
AF Saatchi, Sassan
Marlier, Miriam
Chazdon, Robin L.
Clark, David B.
Russell, Ann E.
TI Impact of spatial variability of tropical forest structure on radar
estimation of aboveground biomass
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Radar; Lidar; Biomass; Carbon; Forest structure; Tropical forests; Costa
Rica; La Selva Biological Station; DESDynI; BIOMASS
ID RAIN-FOREST; LANDSCAPE-SCALE; COSTA-RICA; LIGHT; SAR; LIDAR;
HETEROGENEITY; PLANTATIONS; GROWTH
AB Understanding the spatial variability of tropical forest structure and its impact on the radar estimation of aboveground biomass (AGB) is important to assess the scale and accuracy of mapping AGB with future low frequency radar missions. We used forest inventory plots in old growth, secondary succession, and forest plantations at the La Selva Biological Station in Costa Rica to examine the spatial variability of AGB and its impact on the L-band and P-band polarimetric radar estimation of AGB at multiple spatial scales. Field estimation of AGB was determined from tree size measurements and an allometric equation developed for tropical wet forests. The field data showed very high spatial variability of forest structure with no spatial dependence at a scale above 11 m in old-growth forest. Plot sizes of greater than 0.25 ha reduced the coefficients of variation in AGB to below 20% and yielded a stationary and normal distribution of AGB over the landscape. Radar backscatter measurements at all polarization channels were strongly positively correlated with AGB at three scales of 0.25 ha, 0.5 ha, and 1.0 ha. Among these measurements, PHV and LHV showed strong sensitivity to AGB<300 Mg ha(-1) and AGB<150 Mg ha(-1) respectively at the 1.0 ha scale. The sensitivity varied across forest types because of differences in the effects of forest canopy and gap structure on radar attenuation and scattering. Spatial variability of structure and speckle noise in radar measurements contributed equally to degrading the sensitivity of the radar measurements to AGB at spatial scales less than 1.0 ha. By using algorithms based on polarized radar backscatter, we estimated AGB with RMSE = 22.6 Mg ha(-1) for AGB<300 Mg ha(-1) at P-band and RMSE = 23.8 Mg ha(-1) for AGB<150 Mg ha(-1) at L-band and with the accuracy optimized at 1-ha scale within 95% confidence interval. By adding the forest height, estimated from the C-band Interferometry data as an independent variable to the algorithm, the AGB estimation improved beyond the backscatter sensitivity by 20% at P-band and 40% at L-band. The results suggested the estimation of AGB can be improved substantially from the fusion of lidar or InSAR derived forest height with the polarimetric backscatter. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Marlier, Miriam] Univ Calif Los Angeles, Dept Atmospher Sci, Los Angeles, CA 90095 USA.
[Chazdon, Robin L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA.
[Clark, David B.] Univ Missouri, Int Ctr Trop Ecol, Columbia, MO 65211 USA.
[Russell, Ann E.] Iowa State Univ, Dep Nat Resource Ecol & Management, Ames, IA 50011 USA.
RP Saatchi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM saatchi@congo.jpl.nasa.gov
RI Beckley, Matthew/D-4547-2013;
OI Chazdon, Robin/0000-0002-7349-5687
FU National Aeronautic and Space Administration; DOE; NSF; Andrew W. Mellon
Foundation
FX This work was performed partially at the Jet Propulsion laboratory,
California Institute of Technology, under contract from National
Aeronautic and Space Administration and the support of NASA's
Terrestrial Ecology Program. We would like to thank the NASA AIRSAR crew
for the acquisition of the radar images and the JPL airborne SAR group
for processing and calibration of the data. We thank Dr. Ralph Dubayah
and Bryan Blair and Michele Hofton for their help for processing the
LVIS data. Our special thanks also go to the La Selva Biological
Station, the Organization for Tropical Studies, and the Carbono Project
(funded by DOE, NSF and the Andrew W. Mellon Foundation).
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2836
EP 2849
DI 10.1016/j.rse.2010.07.015
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400009
ER
PT J
AU Le Toan, T
Quegan, S
Davidson, MWJ
Balzter, H
Paillou, P
Papathanassiou, K
Plummer, S
Rocca, F
Saatchi, S
Shugart, H
Ulander, L
AF Le Toan, T.
Quegan, S.
Davidson, M. W. J.
Balzter, H.
Paillou, P.
Papathanassiou, K.
Plummer, S.
Rocca, F.
Saatchi, S.
Shugart, H.
Ulander, L.
TI The BIOMASS mission: Mapping global forest biomass to better understand
the terrestrial carbon cycle
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Forest biomass; Carbon cycle; P-band SAR; Satellite mission; ESA Earth
Explorer
ID POLARIMETRIC SAR INTERFEROMETRY; ORBITAL IMAGING RADAR; TROPICAL
RAIN-FOREST; L-BAND; P-BAND; SPATIAL-DISTRIBUTION; FARADAY-ROTATION;
PINE FOREST; AMAZON; MODEL
AB In response to the urgent need for improved mapping of global biomass and the lack of any current space systems capable of addressing this need, the BIOMASS mission was proposed to the European Space Agency for the third cycle of Earth Explorer Core missions and was selected for Feasibility Study (Phase A) in March 2009. The objectives of the mission are 1) to quantify the magnitude and distribution of forest biomass globally to improve resource assessment, carbon accounting and carbon models, and 2) to monitor and quantify changes in terrestrial forest biomass globally, on an annual basis or better, leading to improved estimates of terrestrial carbon sources (primarily from deforestation); and terrestrial carbon sinks due to forest regrowth and afforestation. These science objectives require the mission to measure above-ground forest biomass from 70 degrees N to 56 degrees Sat spatial scale of 100-200 m, with error not exceeding +/- 20% or +/- 10 t ha(-1) and forest height with error of +/- 4 m. To meet the measurement requirements, the mission will carry a P-Band polarimetric SAR (centre frequency 435 MHz with 6 MHz bandwidth) with interferometric capability, operating in a dawn-dusk orbit with a constant incidence angle (in the range of 25 degrees-35 degrees) and a 25-45 day repeat cycle. During its 5-year lifetime, the mission will be capable of providing both direct measurements of biomass derived from intensity data and measurements of forest height derived from polarimetric interferometry. The design of the BIOMASS mission spins together two main observational strands: (1) the long heritage of airborne observations in tropical, temperate and boreal forest that have demonstrated the capabilities of P-band SAR for measuring forest biomass; (2) new developments in recovery of forest structure including forest height from Pol-InSAR, and, crucially, the resistance of P-band to temporal decorrelation, which makes this frequency uniquely suitable for biomass measurements with a single repeat-pass satellite. These two complementary measurement approaches are combined in the single BIOMASS sensor, and have the satisfying property that increasing biomass reduces the sensitivity of the former approach while increasing the sensitivity of the latter. This paper surveys the body of evidence built up over the last decade, from a wide range of airborne experiments, which illustrates the ability of such a sensor to provide the required measurements.
At present, the BIOMASS P-band radar appears to be the only sensor capable of providing the necessary global knowledge about the world's forest biomass and its changes. In addition, this first chance to explore the Earth's environment with a long wavelength satellite SAR is expected to make yield new information in a range of geoscience areas, including subsurface structure in arid lands and polar ice, and forest inundation dynamics. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Le Toan, T.] Univ Toulouse 3, Ctr Etud Spatiales Biosphere, CNRS, CNES,IRD, F-31062 Toulouse, France.
[Quegan, S.] Univ Sheffield, CTCD, Sheffield S10 2TN, S Yorkshire, England.
[Balzter, H.] Univ Leicester, Ctr Environm Res CERES, Leicester LE1 7RH, Leics, England.
[Paillou, P.] Univ Bordeaux 1, Observ Aquitain Sci Univers, F-33405 Talence, France.
[Papathanassiou, K.] German Aerosp Ctr eV DLR, Wessling, Germany.
[Rocca, F.] Politecn Milan, Dipartimento Elettron & Informaz, Milan, Italy.
[Saatchi, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Shugart, H.] Univ Virginia, Charlottesville, VA USA.
[Ulander, L.] FOI, Dept Radar Syst, Linkoping, Sweden.
RP Le Toan, T (reprint author), Univ Toulouse 3, Ctr Etud Spatiales Biosphere, CNRS, CNES,IRD, F-31062 Toulouse, France.
EM Thuy.Letoan@cesbio.cnes.fr
RI Balzter, Heiko/B-5976-2008
OI Balzter, Heiko/0000-0002-9053-4684
FU European Space Agency; national institutes and agencies
FX The authors, who made up the BIOMASS Phase 0 Mission Assessment Group,
would like to thank the European Space Agency, and their national
institutes and agencies for supporting the work presented in this paper.
NR 91
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2850
EP 2860
DI 10.1016/j.rse.2011.03.020
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400010
ER
PT J
AU Mitchard, ETA
Saatchi, SS
Lewis, SL
Feldpausch, TR
Woodhouse, IH
Sonke, B
Rowland, C
Meir, P
AF Mitchard, E. T. A.
Saatchi, S. S.
Lewis, S. L.
Feldpausch, T. R.
Woodhouse, I. H.
Sonke, B.
Rowland, C.
Meir, P.
TI Measuring biomass changes due to woody encroachment and
deforestation/degradation in a forest-savanna boundary region of central
Africa using multi-temporal L-band radar backscatter
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE ALOS PALSAR; Aboveground biomass; Cameroon; Change detection;
Deforestation; Degradation; Ecotone; Forest-savanna boundary; JERS-1;
SAR; Radar; REDD; Woody encroachment
ID TROPICAL FORESTS; RAIN-FOREST; CENTRAL AMAZONIA; SOIL-MOISTURE;
NATIONAL-PARK; IVORY-COAST; VEGETATION; CARBON; COVER; EXPANSION
AB Satellite L-band synthetic aperture radar backscatter data from 1996 and 2007 (from JERS-1 and ALOS PALSAR respectively), were used with field data collected in 2007 and a back-calibration method to produce biomass maps of a 15 000 km(2) forest-savanna ecotone region of central Cameroon. The relationship between the radar backscatter and aboveground biomass (AGB) was strong (r(2)=0.86 for ALOS HV to biomass plots, r(2)=0.95 relating ALOS-derived biomass for 40 suspected unchanged regions to JERS-1 HH). The root mean square error (RMSE) associated with AGB estimation varied from similar to 25% for AGB<100 Mg ha(-1) to similar to 40% for AGB>100 Mg ha(-1) for the ALOS HV data. Change detection showed a significant loss of AGB over high biomass forests, due to suspected deforestation and degradation, and significant biomass gains along the forest-savanna boundary, particularly in areas of low population density. Analysis of the errors involved showed that radar data can detect changes in broad AGB class in forest-savanna transition areas with an accuracy >95%. However, quantitative assessment of changes in AGB in Mg ha(-1) at a pixel level will require radar images from sensors with similar characteristics collecting data from the same season over multiple years. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Mitchard, E. T. A.; Woodhouse, I. H.; Meir, P.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland.
[Saatchi, S. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lewis, S. L.; Feldpausch, T. R.] Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England.
[Sonke, B.] Univ Yaounde, Dept Biol, Yaounde, Cameroon.
[Rowland, C.] Lancaster Environm Ctr, CEH Lancaster, Lancaster LA1 4AP, England.
RP Mitchard, ETA (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland.
EM edward.mitchard@ed.ac.uk
RI Woodhouse, Iain/B-1790-2009; Lewis, Simon/I-9025-2012; Meir,
Patrick/J-8344-2012; Feldpausch, Ted/D-3436-2009; chen, zhu/K-5923-2013;
OI Feldpausch, Ted/0000-0002-6631-7962; Mitchard,
Edward/0000-0002-5690-4055; Lewis, Simon/0000-0002-8066-6851
FU Gatsby Plants; TROBIT; NERC [NE/D005590/1]; Royal Society
FX The authors would like to acknowledge Gatsby Plants for providing ETAM's
PhD studentship, and TROBIT, a NERC-funded consortium, grant ref:
NE/D005590/1, for funding the rest of the work. SLL was funded by a
Royal Society University Research Fellowship. Jon Lloyd, TROBIT P.I.,
provided useful advice and expertise. Three anonymous referees provided
helpful suggestions and comments on an earlier version of the manuscript
that were instrumental in improving the study. Adam Freedman provided
advice on the sources of accurate population data. Jeanette Sonke,
Wildlife Conservation Society-Cameroon (WCS-Cameroon), The University of
Yaounde I, and 14 canoeists from Mbakaou provided invaluable support in
Cameroon. Remote sensing data were provided by the Alaska Satellite
Facility, the Global Rainforest Mapping Project, NASA and Eurimage;
Landsat and ASTER images were provided free of charge by Terralook,
courtesy of USGS EROS and NASA's Jet Propulsion Laboratory; TRMM 3843
data was downloaded from the Giovanni online data system, developed and
maintained by the NASA Goddard Earth Sciences (GES) Data and Information
Services Center (DISC).
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SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2861
EP 2873
DI 10.1016/j.rse.2010.02.022
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400011
ER
PT J
AU Ahmed, R
Siqueira, P
Hensley, S
Chapman, B
Bergen, K
AF Ahmed, Razi
Siqueira, Paul
Hensley, Scott
Chapman, Bruce
Bergen, Kathleen
TI A survey of temporal decorrelation from spaceborne L-Band repeat-pass
InSAR
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE InSAR; Temporal decorrelation; DESDynI; SIR-C; L-Band
ID SYNTHETIC APERTURE RADARS; STEM VOLUME RETRIEVAL; INTERFEROMETRIC RADAR;
SAR INTERFEROMETRY; BOREAL FORESTS; VEGETATION; BIOMASS; HEIGHT;
TOPOGRAPHY; COHERENCE
AB In this paper we quantify the effects of temporal decorrelation in repeat pass synthetic aperture radar interferometry (InSAR). Temporal decorrelation causes significant uncertainties in vegetation parameter estimates obtained using various InSAR techniques, which are desired on a global scale. Because of its stochastic nature temporal decorrelation is hard to model and isolate. In this paper we analyze temporal decorrelation statistically as observed in a large swath of SIR-C L-Band InSAR data collected over the eastern United States, with a repeat pass duration of one day in October 1994 and a near zero perpendicular baseline. The very small baseline for this particular pair makes the effect of volumetric scattering on correlation magnitude statistics nearly imperceptible, allowing for a quantitative analysis of temporal effects alone. The swath analyzed in this paper spans more than a million hectares of terrain comprised primarily of deciduous and evergreen forests, agricultural land, water and urban areas. The relationships of these different land-cover types, phenology and weather conditions (i.e. precipitation and wind) on the measures of interferometric correlation is analyzed in what amounts to be the most geographically extensive analysis of this phenomenon to date. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Ahmed, Razi; Siqueira, Paul] Univ Massachusetts, Dept Elect & Comp Engn, Amherst, MA 01003 USA.
[Hensley, Scott; Chapman, Bruce] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bergen, Kathleen] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA.
RP Siqueira, P (reprint author), Univ Massachusetts, Dept Elect & Comp Engn, Amherst, MA 01003 USA.
EM ahmed@mirsl.ecs.umass.edu; siqueira@ecs.umass.edu
RI chen, zhu/K-5923-2013; Siqueira, Paul/D-9760-2016
OI Siqueira, Paul/0000-0001-5781-8282
NR 34
TC 25
Z9 25
U1 2
U2 25
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 NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2887
EP 2896
DI 10.1016/j.rse.2010.03.017
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400013
ER
PT J
AU Sun, GQ
Ranson, KJ
Guo, Z
Zhang, Z
Montesano, P
Kimes, D
AF Sun, Guoqing
Ranson, K. Jon
Guo, Z.
Zhang, Z.
Montesano, P.
Kimes, D.
TI Forest biomass mapping from lidar and radar synergies
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Forest biomass; DESDynI mission; Lidar waveform; LVIS; SRTM; PALSAR;
InSAR; SRTM
ID SIR-C/X-SAR; TOPOGRAPHY MISSION; MANGROVE FORESTS; TROPICAL FOREST;
ELEVATION DATA; VEGETATION; BACKSCATTER; HEIGHT; INTERFEROMETRY;
ICESAT/GLAS
AB The use of lidar and radar instruments to measure forest structure attributes such as height and biomass at global scales is being considered for a future Earth Observation satellite mission, DESDynI (Deformation, Ecosystem Structure, and Dynamics of Ice). Large footprint lidar makes a direct measurement of the heights of scatterers in the illuminated footprint and can yield accurate information about the vertical profile of the canopy within lidar footprint samples. Synthetic Aperture Radar (SAR) is known to sense the canopy volume, especially at longer wavelengths and provides image data. Methods for biomass mapping by a combination of lidar sampling and radar mapping need to be developed.
In this study, several issues in this respect were investigated using aircraft borne lidar and SAR data in Howland, Maine, USA. The stepwise regression selected the height indices rh50 and rh75 of the Laser Vegetation Imaging Sensor (LVIS) data for predicting field measured biomass with a R(2) of 0.71 and RMSE of 3133 Mg/ha. The above-ground biomass map generated from this regression model was considered to represent the true biomass of the area and was used as a reference map since no better biomass map exists for the area. Random samples were taken from the biomass map and the correlation between the sampled biomass and co-located SAR signature was studied. The best models were used to extend the biomass from lidar samples into all forested areas in the study area, which mimics a procedure that could be used for the future DESDYnI mission. It was found that depending on the data types used (quad-pol or dual-pol) the SAR data can predict the lidar biomass samples with R(2) of 0.63-0.71. RMSE of 32.0-28.2 Mg/ha up to biomass levels of 200-250 Mg/ha. The mean biomass of the study area calculated from the biomass maps generated by lidar-SAR synergy was within 10% of the reference biomass map derived from LVIS data. The results from this study are preliminary, but do show the potential of the combined use of lidar samples and radar imagery for forest biomass mapping. Various issues regarding lidar/radar data synergies for biomass mapping are discussed in the paper. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Sun, Guoqing] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Ranson, K. Jon; Kimes, D.] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Guo, Z.] Chinese Acad Sci, State Key Lab Remote Sensing, Inst Remote Sensing Applicat, Beijing 100101, Peoples R China.
[Zhang, Z.] Beijing Normal Univ, Sch Geog, Beijing 100875, Peoples R China.
[Montesano, P.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Sun, GQ (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
EM guoqing.sun@gmail.com
RI Ranson, Kenneth/G-2446-2012; chen, zhu/K-5923-2013; Beckley,
Matthew/D-4547-2013
OI Ranson, Kenneth/0000-0003-3806-7270;
FU National Basic Research Program of China [2007CB714404]; National
Natural Science Foundation of China [40701124, 40734025]; NASA Remote
Sensing Science [NNG06G133G]; Terrestrial Ecology Program [NNX09AG66G];
University of Maryland, College Park; NASA [NAG512112]
FX The support to Chinese contributors was from National Basic Research
Program of China (Grant no. 2007CB714404) and National Natural Science
Foundation of China (Grant nos. 40701124, 40734025). Major work was
supported by NASA Remote Sensing Science (grant number NNG06G133G) and
Terrestrial Ecology Program (NNX09AG66G). The LVIS data sets were
provided by the Laser Vegetation Imaging Sensor (LVIS) team in the Laser
Remote Sensing Branch at NASA Goddard Space Flight Center with support
from the University of Maryland, College Park. Funding for the
collection and processing of the 2003 Northeastern USA data was provided
by NASA's Terrestrial Ecology Program (NASA Grant number NAG512112).
ALOS PALSAR data were provided by JAXA EORC. Dr. Joanne Howl assisted
with final edits of the manuscript.
NR 50
TC 54
Z9 61
U1 7
U2 76
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 NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2906
EP 2916
DI 10.1016/j.rse.2011.03.021
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400015
ER
PT J
AU Swatantran, A
Dubayah, R
Roberts, D
Hofton, M
Blair, JB
AF Swatantran, Anu
Dubayah, Ralph
Roberts, Dar
Hofton, Michelle
Blair, J. Bryan
TI Mapping biomass and stress in the Sierra Nevada using lidar and
hyperspectral data fusion
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE LVIS; AVIRIS; Lidar; Hyperspectral; Biomass; MESMA; Species; Stress
ID SPECTRAL MIXTURE ANALYSIS; LARGE-FOOTPRINT LIDAR; MIXED-CONIFER FOREST;
WAVE-FORM LIDAR; LEAF-AREA INDEX; IMAGING SPECTROMETER; RAIN-FOREST;
LASER ALTIMETER; WATER STATUS; ETM PLUS
AB In this paper, we explored fusion of structural metrics from the Laser Vegetation Imaging Sensor (LVIS) and spectral characteristics from the Airborne Visible Infrared Imaging Spectrometer (AVIRIS) for biomass estimation in the Sierra Nevada. in addition, we combined the two sensors to map species-specific biomass and stress at landscape scale. Multiple endmember spectral mixture analysis (MESMA) was used to classify vegetation from AVIRIS images and obtain sub-pixel fractions of green vegetation, non-photosynthetic vegetation, soil, and shade.,LVIS metrics. AVIRIS spectral indices, and MESMA fractions were compared with field measures of biomass using linear and stepwise regressions at stand (1 ha) level. AVIRIS metrics such as water band indices and shade fractions showed strong correlation with LVIS canopy height (r(2) = 0.69, RMSE = 5.2 m) and explained around 60% variability in biomass. LVIS variables were found to be consistently good predictors of total and species specific biomass (r(2) = 0.77, RMSE = 70.12 Mg/ha). Prediction by LVIS after species stratification of field data reduced errors by 12% (r(2) = 0.84. RMSE = 58.78 Mg/ha) over using LVIS metrics alone. Species-specific biomass maps and associated errors created from fusion were different from those produced without fusion, particularly for hardwoods and pines, although mean biomass differences between the two techniques were not statistically significant. A combined analysis of spatial maps from LVIS and AVIRIS showed increased water and chlorophyll stress in several high biomass stands in the study area. This study provides further evidence that lidar is better suited for biomass estimation, per se, while the best use of hyperspectral data may be to refine biomass predictions through a priori species stratification, while also providing information on canopy state, such as stress. Together, the two sensors have many potential applications in carbon dynamics, ecological and habitat studies. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Swatantran, Anu; Dubayah, Ralph; Hofton, Michelle] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Roberts, Dar] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Blair, J. Bryan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Swatantran, A (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
EM aswatan@umd.edu
RI Khachadourian, Diana/C-8513-2012; Blair, James/D-3881-2013; Beckley,
Matthew/D-4547-2013; Swatantran, Anu/B-8786-2016
FU Multisite Integration of LIDAR and Hyperspectral Data for Improved
Estimation of Carbon Stocks and Exchanges; NASA [NNG05GE56G, NNX06AF91H]
FX This research was funded in part by "Multisite Integration of LIDAR and
Hyperspectral Data for Improved Estimation of Carbon Stocks and
Exchanges" (P.I. Dar Roberts), NASA Carbon Cycle Science grant
(NNG05GE56G) and a NASA Earth and Space Science graduate fellowship
(NNX06AF91H). Error matrix codes for assessing accuracy of MESMA models
were made available by Phillip Dennsion. We are thankful to Kerry
Halligan, Dylan Parenti and the Viper Lab team at University of
California, Santa Barbara for software training and help with AVIRIS
data processing. We thank Peter Hyde for providing useful inputs from
previous studies in the Sierra Nevada.
NR 69
TC 64
Z9 68
U1 6
U2 70
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 NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2917
EP 2930
DI 10.1016/j.rse.2010.08.027
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400016
ER
PT J
AU Chopping, M
Schaaf, CB
Zhao, F
Wang, ZS
Nolin, AW
Moisen, GG
Martonchik, JV
Bull, M
AF Chopping, Mark
Schaaf, Crystal B.
Zhao, Feng
Wang, Zhuosen
Nolin, Anne W.
Moisen, Gretchen G.
Martonchik, John V.
Bull, Michael
TI Forest structure and aboveground biomass in the southwestern United
States from MODIS and MISR
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Earth Observing System; Forest; Structure; Biomass; Carbon; Disturbance;
Multi-angle; BRDF; Modeling; Land cover; Moderate resolution
ID REMOTE-SENSING DATA; ANGLE SPECTRAL DATA; REFLECTANCE MODEL;
BIDIRECTIONAL REFLECTANCE; VERTICAL STRUCTURE; CANOPY; VEGETATION;
SURFACE; COVER; INVARIANTS
AB Red band bidirectional reflectance factor data from the NASA MODerate resolution Imaging Spectro-radiometer (MODIS) acquired over the southwestern United States were interpreted through a simple geometric-optical (GO) canopy reflectance model to provide maps of fractional crown cover (dimensionless), mean canopy height (m), and aboveground woody biomass (Mg ha(-1)) on a 250 m grid. Model adjustment was performed after dynamic injection of a background contribution predicted via the kernel weights of a bidirectional reflectance distribution function (BRDF) model. Accuracy was assessed with respect to similar maps obtained with data from the NASA Multiangle Imaging Spectroradiometer (MISR) and to contemporaneous US Forest Service (USFS) maps based partly on Forest Inventory and Analysis (FIA) data. MODIS and MISR retrievals of forest fractional cover and mean height both showed compatibility with the USFS maps, with MODIS mean absolute errors (MAE) of 0.09 and 8.4 m respectively, compared with MISR MAE of 0.10 and 2.2 m, respectively. The respective MAE for aboveground woody biomass was similar to 10 Mg ha(-1), the same as that from MISR, although the MODIS retrievals showed a much weaker correlation, noting that these statistics do not represent evaluation with respect to ground survey data. Good height retrieval accuracies with respect to averages from high resolution discrete return lidar data and matches between mean crown aspect ratio and mean crown radius maps and known vegetation type distributions both support the contention that the GO model results are not spurious when adjusted against MISR bidirectional reflectance factor data. These results highlight an alternative to empirical methods for the exploitation of moderate resolution remote sensing data in the mapping of woody plant canopies and assessment of woody biomass loss and recovery from disturbance in the southwestern United States and in parts of the world where similar environmental conditions prevail. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Chopping, Mark] Montclair State Univ, Montclair, NJ 07043 USA.
[Schaaf, Crystal B.; Zhao, Feng; Wang, Zhuosen] Boston Univ, Ctr Remote Sensing, Boston, MA 02215 USA.
[Nolin, Anne W.] Oregon State Univ, Dept Geosci, Corvallis, OR 97331 USA.
[Moisen, Gretchen G.] Forest Serv, USDA, Rocky Mt Res Stn, Ogden, UT 84401 USA.
[Martonchik, John V.; Bull, Michael] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chopping, M (reprint author), Montclair State Univ, 1 Normal Ave, Montclair, NJ 07043 USA.
EM chopping@pegasus.montclair.edu
RI Beckley, Matthew/D-4547-2013
FU NASA [NNX08AE71G]
FX This research was supported by NASA Earth Observing System grant
NNX08AE71G to MC (Technical Manager: Dr. Diane Wickland). The MISR and
MODIS data were obtained from the NASA Langley Atmospheric Science Data
Center and the NASA EOS Data Gateway, respectively. We thank Xiaohong
Chopping, David Diner (MISR Scientist, NASA/JPL), Jock Blackard and Ron
Tymcio (US Forest Service, Rocky Mountain Research Station, Ogden, UT),
Matt Smith and the Global Land Cover Facility (University of Maryland,
College Park, MD), Barbara Nolen (Jornada Long Term Ecological
Research), Joseph Youn and Michael Stoppay (Computer Operations for
Research and Education, College of Science and Mathematics, Montclair
State University), and the three anonymous reviewers.
NR 63
TC 21
Z9 23
U1 3
U2 37
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 NOV 15
PY 2011
VL 115
IS 11
SI SI
BP 2943
EP 2953
DI 10.1016/j.rse.2010.08.031
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 828LB
UT WOS:000295501400018
ER
PT J
AU Whiteman, DN
Vermeesch, KC
Oman, LD
Weatherhead, EC
AF Whiteman, David N.
Vermeesch, Kevin C.
Oman, Luke D.
Weatherhead, Elizabeth C.
TI The relative importance of random error and observation frequency in
detecting trends in upper tropospheric water vapor
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RAMAN LIDAR; AWEX-G; CLIMATE; VALIDATION; SYSTEM
AB Recent published work assessed the amount of time to detect trends in atmospheric water vapor over the coming century. We address the same question and conclude that under the most optimistic scenarios and assuming perfect data (i.e., observations with no measurement uncertainty) the time to detect trends will be at least 12 years at approximately 200 hPa in the upper troposphere. Our times to detect trends are therefore shorter than those recently reported and this difference is affected by data sources used, method of processing the data, geographic location and pressure level in the atmosphere where the analyses were performed. We then consider the question of how instrumental uncertainty plays into the assessment of time to detect trends. We conclude that due to the high natural variability in atmospheric water vapor, the amount of time to detect trends in the upper troposphere is relatively insensitive to instrumental random uncertainty and that it is much more important to increase the frequency of measurement than to decrease the random error in the measurement. This is put in the context of international networks such as the Global Climate Observing System (GCOS) Reference Upper-Air Network (GRUAN) and the Network for the Detection of Atmospheric Composition Change (NDACC) that are tasked with developing time series of climate quality water vapor data.
C1 [Whiteman, David N.; Vermeesch, Kevin C.; Oman, Luke D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Weatherhead, Elizabeth C.] Univ Colorado, CIRES GSD, Boulder, CO 80305 USA.
[Vermeesch, Kevin C.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Whiteman, DN (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM david.n.whiteman@nasa.gov
RI Oman, Luke/C-2778-2009; Weatherhead, Elizabeth/I-7091-2015
OI Oman, Luke/0000-0002-5487-2598; Weatherhead,
Elizabeth/0000-0002-9252-4228
FU NASA
FX We would like to acknowledge the NASA Atmospheric Composition program
for support of this work. We acknowledge the U. S. Department of
Energy's Atmospheric Radiation Measurements program for the radiosonde
and lidar data used here. We also greatly acknowledge the useful
comments and suggestions made by Reinout Boers and Tom Gardiner.
NR 25
TC 17
Z9 17
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD NOV 12
PY 2011
VL 116
AR D21118
DI 10.1029/2011JD016610
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 848KZ
UT WOS:000297051800008
ER
PT J
AU Kwok, R
Panzer, B
Leuschen, C
Pang, S
Markus, T
Holt, B
Gogineni, S
AF Kwok, R.
Panzer, B.
Leuschen, C.
Pang, S.
Markus, T.
Holt, B.
Gogineni, S.
TI Airborne surveys of snow depth over Arctic sea ice
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID OCEAN; THICKNESS; LASER
AB During the spring of 2009, an ultrawideband microwave radar was deployed as part of Operation IceBridge to provide the first cross-basin surveys of snow thickness over Arctic sea ice. In this paper, we analyze data from three similar to 2000 km transects to examine detection issues, the limitations of the current instrument, and the regional variability of the retrieved snow depth. Snow depth is the vertical distance between the air-snow and snow-ice interfaces detected in the radar echograms. Under ideal conditions, the per echogram uncertainty in snow depth retrieval is similar to 4-5 cm. The finite range resolution of the radar (similar to 5 cm) and the relative amplitude of backscatter from the two interfaces limit the direct retrieval of snow depths much below similar to 8 cm. Well-defined interfaces are observed over only relatively smooth surfaces within the radar footprint of similar to 6.5 m. Sampling is thus restricted to undeformed, level ice. In early April, mean snow depths are 28.5 +/- 16.6 cm and 41.0 +/- 22.2 cm over first-year and multiyear sea ice (MYI), respectively. Regionally, snow thickness is thinner and quite uniform over the large expanse of seasonal ice in the Beaufort Sea, and gets progressively thicker toward the MYI cover north of Ellesmere Island, Greenland, and the Fram Strait. Snow depth over MYI is comparable to that reported in the climatology by Warren et al. (1999). Ongoing improvements to the radar system and the utility of these snow depth measurements are discussed.
C1 [Kwok, R.; Pang, S.; Holt, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Panzer, B.; Leuschen, C.; Gogineni, S.] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66046 USA.
[Markus, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ron.kowk@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU NASA; NSF
FX The QuikSCAT data are provided by the Physical Oceanography DAAC at the
Jet Propulsion Laboratory, Pasadena, California. The IceBridge snow
radar data are provided by the National Snow and Ice Data Center. The
snow radar development was carried out by CReSIS with support from NASA
and NSF. R.K., S.P., and B.H. carried out this work at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 17
TC 21
Z9 21
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-OCEANS
JI J. Geophys. Res.-Oceans
PD NOV 12
PY 2011
VL 116
AR C11018
DI 10.1029/2011JC007371
PG 16
WC Oceanography
SC Oceanography
GA 848RY
UT WOS:000297072800005
ER
PT J
AU Bell, JM
Bougher, SW
Waite, JH
Ridley, AJ
Magee, BA
Mandt, KE
Westlake, J
DeJong, AD
Bar-Nun, A
Jacovi, R
Toth, G
De la Haye, V
Gell, D
Fletcher, G
AF Bell, Jared M.
Bougher, Stephen W.
Waite, J. Hunter, Jr.
Ridley, Aaron J.
Magee, Brian A.
Mandt, Kathleen E.
Westlake, Joseph
DeJong, Anna D.
Bar-Nun, Akiva
Jacovi, Ronen
Toth, Gabor
De la Haye, Virginie
Gell, David
Fletcher, Gregory
TI Simulating the one-dimensional structure of Titan's upper atmosphere: 3.
Mechanisms determining methane escape
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MODEL; SPECTROMETER; AEROSOLS; ION; HCN
AB This investigation extends the work presented by Bell et al. (2010a, 2010b). Using the one-dimensional (1-D) configuration of the Titan Global Ionosphere-Thermosphere Model (T-GITM), we quantify the relative importance of the different dynamical and chemical mechanisms that determine the CH4 escape rates calculated by T-GITM. Moreover, we consider the implications of updated Huygens Gas Chromatograph Mass Spectrometer (GCMS) determinations of both the Ar-40 mixing ratios and N-15/N-14 isotopic ratios in work by Niemann et al. (2010). Combining the GCMS constraints in the lower atmosphere with the Ion Neutral Mass Spectrometer (INMS) measurements in work by Magee et al. (2009), our simulation results suggest that the optimal CH4 homopause altitude is located at 1000 km. Using this homopause altitude, we conclude that topside escape rates of 1.0 x 10(10) CH4 m(-2) s(-1) (referred to the surface) are sufficient to reproduce the INMS methane measurements in work by Magee et al. (2009). These escape rates of methane are consistent with the upper limits to methane escape (1.11 x 10(11) CH4 m(-2) s(-1)) established by both the Cassini Plasma Spectrometer (CAPS) and Magnetosphere Imaging Instrument (MIMI) measurements of Carbon-group ions in the near Titan magnetosphere.
C1 [Bell, Jared M.; Waite, J. Hunter, Jr.; Magee, Brian A.; Mandt, Kathleen E.; DeJong, Anna D.; De la Haye, Virginie; Gell, David; Fletcher, Gregory] SW Res Inst, Div Space Sci & Engn, San Antonio, TX 78228 USA.
[Bougher, Stephen W.; Ridley, Aaron J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Mandt, Kathleen E.] Univ Texas San Antonio, Dept Civil & Environm Engn, San Antonio, TX 78249 USA.
[Westlake, Joseph] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA.
[Bar-Nun, Akiva] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel.
[Jacovi, Ronen] CALTECH, Jet Prop Lab, Ice Spect Lab, Pasadena, CA 91109 USA.
RP Bell, JM (reprint author), SW Res Inst, Div Space Sci & Engn, 6220 Culebra Rd,POB 28510, San Antonio, TX 78228 USA.
EM jbell@swri.edu
RI Toth, Gabor/B-7977-2013; Bougher, Stephen/C-1913-2013; Mandt,
Kathleen/M-9812-2013; Ridley, Aaron/F-3943-2011; Westlake,
Joseph/G-2732-2015
OI Toth, Gabor/0000-0002-5654-9823; Bougher, Stephen/0000-0002-4178-2729;
Mandt, Kathleen/0000-0001-8397-3315; Ridley, Aaron/0000-0001-6933-8534;
Westlake, Joseph/0000-0003-0472-8640
FU NASA through Jet Propulsion Laboratory (JPL) [NAS703001NM0710023]
FX This work was supported by the NASA grant NAS703001NM0710023,
subcontracted through the Jet Propulsion Laboratory (JPL). J. Bell would
also like to thank the Center for Space Environment Modeling (CSEM) at
the University of Michigan for continued access and use of their
computational facilities and expertise. Lastly, the authors thank the
staff at both the NASA High End Computing (HEC) and the Texas Advanced
Computing Center (TACC) for use of their large scale computing
facilities.
NR 32
TC 13
Z9 13
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD NOV 12
PY 2011
VL 116
AR E11002
DI 10.1029/2010JE003639
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 848JD
UT WOS:000297046900001
ER
PT J
AU Davies, AG
Keszthelyi, L
McEwen, AS
AF Davies, Ashley Gerard
Keszthelyi, Laszlo
McEwen, Alfred S.
TI Estimating eruption temperature from thermal emission spectra of lava
fountain activity in the Erta'Ale (Ethiopia) volcano lava lake:
Implications for observing Io's volcanoes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SIGNATURE; INTERIOR; PELE
AB We have analysed high-spatial-resolution and high-temporal-resolution temperature measurements of the active lava lake at Erta'Ale volcano, Ethiopia, to derive requirements for measuring eruption temperatures at Io's volcanoes. Lava lakes are particularly attractive targets because they are persistent in activity and large, often with ongoing lava fountain activity that exposes lava at near-eruption temperature. Using infrared thermography, we find that extracting useful temperature estimates from remote-sensing data requires (a) high spatial resolution to isolate lava fountains from adjacent cooler lava and (b) rapid acquisition of multi-color data. Because existing spacecraft data of Io's volcanoes do not meet these criteria, it is particularly important to design future instruments so that they will be able to collect such data. Near-simultaneous data at more than two relatively short wavelengths (shorter than 1 mu m) are needed to constrain eruption temperatures. Resolving parts of the lava lake or fountains that are near the eruption temperature is also essential, and we provide a rough estimate of the required image scale. Citation: Davies, A. G., L. Keszthelyi, and A. S. McEwen (2011), Estimating eruption temperature from thermal emission spectra of lava fountain activity in the Erta'Ale (Ethiopia) volcano lava lake: Implications for observing Io's volcanoes, Geophys. Res. Lett., 38, L21308, doi:10.1029/2011GL049418.
C1 [Davies, Ashley Gerard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Keszthelyi, Laszlo] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ashley.davies@jpl.nasa.gov; laz@usgs.gov; mcewen@lpl.arizona.edu
FU NASA; Jet Propulsion Laboratory-California Institute of Technology
FX This work was carried out at the Jet Propulsion Laboratory-California
Institute of Technology, under contract to NASA. AGD gratefully
acknowledges the support of the NASA Planetary Geology and Geophysics
Program and logistical support from the BBC. ASM and LPK acknowledge the
support of the NASA Planetary Instrument Definition and Development
Program. We thank David Williams and Jani Radebaugh for their reviews.
NR 18
TC 8
Z9 8
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 NOV 11
PY 2011
VL 38
AR L21308
DI 10.1029/2011GL049418
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 848BL
UT WOS:000297021700002
ER
PT J
AU Volkov, DL
Fu, LL
AF Volkov, Denis L.
Fu, Lee-Lueng
TI Interannual variability of the Azores Current strength and eddy energy
in relation to atmospheric forcing
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID NORTH-ATLANTIC OCEAN; SUBTROPICAL GYRE; ALTIMETER DATA; FRONT; FIELD;
TOPEX/POSEIDON; CIRCULATION; GEOSAT; FLOW; COUNTERCURRENT
AB Spaceborne observations of sea surface topography have revealed a significant interannual variability of the Azores Current strength and eddy energy. The objective of this paper is to establish the relationship between these variations and atmospheric forcing over the subtropical North Atlantic. Based on satellite altimetry, hydrography, and atmospheric reanalysis products, it is demonstrated that the interannual variability of the Azores Current eastward velocity and eddy energy may be driven by the adjustment of the ocean to the strength of westerly and trade winds, modulated by the North Atlantic Oscillation. Surface intensification (frontogenesis), which is mainly due to the wind-driven meridional Ekman current convergence, is found significant, but not sufficient to explain the observed interannual variability of the Azores Current strength.
C1 [Volkov, Denis L.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Fu, Lee-Lueng] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Volkov, DL (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, 9258 Boelter Hall,Box 957228, Los Angeles, CA 90095 USA.
EM denis.volkov@jpl.nasa.gov
RI Volkov, Denis/A-6079-2011
OI Volkov, Denis/0000-0002-9290-0502
FU NASA; CNES (Centre National d'Etudes Spatiales, Toulouse, France);
Government sponsorship
FX This research was carried out at Jet Propulsion Laboratory, California
Institute of Technology, and sponsored by the NASA Physical Oceanography
program. MSLA/MDT_CNES-CLS09 are produced by Ssalto-Duacs/C.L.S. Space
Oceanography Division and distributed by Aviso (www.aviso.oceanobs.com)
with support from CNES (Centre National d'Etudes Spatiales, Toulouse,
France). Government sponsorship is acknowledged.
NR 36
TC 5
Z9 6
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-OCEANS
JI J. Geophys. Res.-Oceans
PD NOV 11
PY 2011
VL 116
AR C11011
DI 10.1029/2011JC007271
PG 12
WC Oceanography
SC Oceanography
GA 848RU
UT WOS:000297072400004
ER
PT J
AU Alvarez-Muniz, J
Romero-Wolf, A
Zas, E
AF Alvarez-Muniz, Jaime
Romero-Wolf, Andres
Zas, Enrique
TI Practical and accurate calculations of Askaryan radiation
SO PHYSICAL REVIEW D
LA English
DT Article
ID RAY AIR-SHOWERS; RADIO-EMISSION; NEUTRINO DETECTION; ENERGY NEUTRINOS;
CONDENSED MEDIA; PAIR PRODUCTION; PULSES; CHARGE; BREMSSTRAHLUNG;
SIMULATIONS
AB An in-depth characterization of coherent radio Cherenkov pulses from particle showers in dense dielectric media, referred to as the Askaryan effect, is presented. The time-domain calculation developed in this article is based on a form factor to account for the lateral dimensions of the shower. It is computationally efficient and able to reproduce the results of detailed particle shower simulations with high fidelity in most regions of practical interest, including Fresnel effects due to the longitudinal development of the shower. In addition, an intuitive interpretation of the characteristics of the Askaryan pulse is provided. We expect our approach to benefit the analysis of radio pulses in experiments exploiting the radio technique.
C1 [Alvarez-Muniz, Jaime; Zas, Enrique] Univ Santiago de Compostela, Depto Fis Particulas, Santiago De Compostela 15782, Spain.
[Alvarez-Muniz, Jaime; Zas, Enrique] Univ Santiago de Compostela, Inst Galego Fis Altas Enerxias, Santiago De Compostela 15782, Spain.
[Romero-Wolf, Andres] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Alvarez-Muniz, J (reprint author), Univ Santiago de Compostela, Depto Fis Particulas, Santiago De Compostela 15782, Spain.
RI Alvarez-Muniz, Jaime/H-1857-2015; zas, enrique/I-5556-2015
OI Alvarez-Muniz, Jaime/0000-0002-2367-0803; zas,
enrique/0000-0002-4430-8117
FU Feder, Spain; NASA [NNX07AO05H]; National Aeronautics and Space
Administration
FX J. A-M. and E. Z. thank Xunta de Galicia (INCITE09 206 336 PR) and
Conselleria de Educacion (Grupos de Referencia Competitivos-Consolider
Xunta de Galicia 2006/51); Ministerio de Ciencia e Innovacion (FPA
2007-65114, FPA 2008-01177 and Consolider CPAN-Ingenio 2010) and Feder
Funds, Spain. We thank CESGA (Centro de SuperComputacion de Galicia) for
computing resources and assistance. A. R-W. thanks NASA (NESSF Grant
NNX07AO05H). 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 J. Bray, P.
Gorham, C. W. James, and W. R. Carvalho Jr. for helpful discussions.
NR 58
TC 10
Z9 10
U1 0
U2 1
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD NOV 11
PY 2011
VL 84
IS 10
AR 103003
DI 10.1103/PhysRevD.84.103003
PG 12
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 846PK
UT WOS:000296915500001
ER
PT J
AU Morabito, DD
Verkhoglyadova, OP
Han, D
Riedel, JE
AF Morabito, David D.
Verkhoglyadova, Olga P.
Han, Dongsuk
Riedel, Joseph E.
TI The effects of earthward directed interplanetary coronal mass ejections
on near-Earth S band signal links
SO RADIO SCIENCE
LA English
DT Article
ID LOW-LATITUDE IONOSPHERE; SOLAR-WIND; MAGNETIC STORMS; ELECTRIC-FIELD;
PENETRATION; PREDICTIONS; PHASE; SPEED
AB Human space exploration is expected to enter its next phase in the coming decades as the United States prepares to return to the Moon or perhaps venture even further with a crewed mission to a near-Earth asteroid. Both mission classes are viewed by NASA as precursors of eventual crewed missions to Mars. In anticipation of extensive robotic and human presence in the space environment beyond the protection of the Earth's magnetosphere, it is important to better quantify and bound effects of earthward directed solar storms not just on the human body but also on engineering signals. In this paper, we study the effects of solar storms on S band (similar to 2.3 GHz) radio links in the near-Earth environment, primarily for application to navigation. In particular, we are concerned with induced long-period signatures on Doppler tracking data that could be confused with the Earth's gravity signature, resulting in perturbed trajectory solutions of returning spacecraft during Earth entry targeting. We have quantified "worst-case" levels of such induced signatures on S band signal phase using model predictions based on measured in situ charged particle content from satellites and have compared these results with signatures seen in actual tracking data during periods of interplanetary coronal mass ejections (ICME) and related geomagnetic storms. We show that induced Doppler can mask Earth gravity field effects in navigation trajectory solutions at S band, a commonly used frequency for near-Earth communications and navigation. Finally, we suggest a few ways that such effects can be identified, alleviated or eliminated in near real-time.
C1 [Morabito, David D.; Verkhoglyadova, Olga P.; Han, Dongsuk; Riedel, Joseph E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Morabito, DD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM david.d.morabito@jpl.nasa.gov
OI Verkhoglyadova, Olga/0000-0002-9295-9539
FU NASA; Jet Propulsion Laboratory (JPL) Division; National Aeronautics and
Space Administration
FX We would like to thank the NASA Constellation Project for supporting the
initial phase of this work, and the Jet Propulsion Laboratory (JPL)
Division 300 Raise the Bar (RTB) Program (Stephen Lichten, Peter
Theisinger and Adriana Wall) for supporting an intermediate phase of
this work. We would like to thank Charles Naudet of the Advanced
Engineering Program at JPL for supporting the concluding phase of this
work. We would like to thank Anthony Mannucci of JPL for his valuable
comments on an early draft; Tom Runge and Attila Komjathy of JPL for
assistance in providing TSAC ionospheric calibrations (GIMCAL) used to
adjust Genesis tracking data; and Roger Wiens and the Los Alamos Genesis
Science Team for providing the Genesis particle detector data used in
the correlative analysis discussed in this article. 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. Government
sponsorship acknowledged.
NR 44
TC 0
Z9 0
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
J9 RADIO SCI
JI Radio Sci.
PD NOV 11
PY 2011
VL 46
AR RS6001
DI 10.1029/2011RS004718
PG 13
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 848HU
UT WOS:000297043300002
ER
PT J
AU Lebron-Colon, M
Meador, MA
Lukco, D
Sola, F
Santos-Perez, J
McCorkle, LS
AF Lebron-Colon, M.
Meador, M. A.
Lukco, D.
Sola, F.
Santos-Perez, J.
McCorkle, L. S.
TI Surface oxidation study of single wall carbon nanotubes
SO NANOTECHNOLOGY
LA English
DT Article
ID EPOXY COMPOSITES; POLYMER MATRIX; PURIFICATION; FUNCTIONALIZATION;
DISSOLUTION; DIAMETER; SOLVENTS; GROWTH; TUBES
AB Functionalization of single wall carbon nanotubes (SWCNTs) is desirable to enhance their ability to be incorporated into polymers and enhance their bonding with the matrix. One approach to carbon nanotube functionalization is by oxidation via a strong oxidizing agent or refluxing in strong acids. However, this approach can damage the nanotubes, leading to the introduction of defects and/or shorter nanotubes. Such damage can adversely affect the mechanical, thermal, and electrical properties. A more benign approach to nanotube functionalization has been developed involving photo-oxidation. Chemical analysis by XPS revealed that the oxygen content of the photo-oxidized SWCNTs was 11.3 at.% compared to 6.7 at.% for SWCNTs oxidized by acid treatment. The photo-oxidized SWCNTs produced by this method can be used directly in various polymer matrices or can be further modified by additional chemical reactions.
C1 [Lebron-Colon, M.; Lukco, D.] NASA, ASRC Aerosp Corp, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Santos-Perez, J.; McCorkle, L. S.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
RP Lebron-Colon, M (reprint author), NASA, ASRC Aerosp Corp, Glenn Res Ctr, 21000 Brookpk Rd,MS 49-1, Cleveland, OH 44135 USA.
EM Marisabel.Lebron-Colon-1@nasa.gov
NR 42
TC 6
Z9 6
U1 0
U2 16
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
EI 1361-6528
J9 NANOTECHNOLOGY
JI Nanotechnology
PD NOV 11
PY 2011
VL 22
IS 45
AR 455707
DI 10.1088/0957-4484/22/45/455707
PG 5
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 844MC
UT WOS:000296750300017
PM 22020272
ER
PT J
AU Chen, Y
Randerson, JT
Morton, DC
DeFries, RS
Collatz, GJ
Kasibhatla, PS
Giglio, L
Jin, YF
Marlier, ME
AF Chen, Yang
Randerson, James T.
Morton, Douglas C.
DeFries, Ruth S.
Collatz, G. James
Kasibhatla, Prasad S.
Giglio, Louis
Jin, Yufang
Marlier, Miriam E.
TI Forecasting Fire Season Severity in South America Using Sea Surface
Temperature Anomalies
SO SCIENCE
LA English
DT Article
ID CLIMATE-CHANGE; AMAZON BASIN; EL-NINO; DEFORESTATION; RAINFALL; FORESTS;
DROUGHT; PRODUCTS; PRECIPITATION; OSCILLATION
AB Fires in South America cause forest degradation and contribute to carbon emissions associated with land use change. We investigated the relationship between year-to-year changes in fire activity in South America and sea surface temperatures. We found that the Oceanic Nino Index was correlated with interannual fire activity in the eastern Amazon, whereas the Atlantic Multidecadal Oscillation index was more closely linked with fires in the southern and southwestern Amazon. Combining these two climate indices, we developed an empirical model to forecast regional fire season severity with lead times of 3 to 5 months. Our approach may contribute to the development of an early warning system for anticipating the vulnerability of Amazon forests to fires, thus enabling more effective management with benefits for climate and air quality.
C1 [Chen, Yang; Randerson, James T.; Jin, Yufang] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Morton, Douglas C.; Collatz, G. James] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[DeFries, Ruth S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Kasibhatla, Prasad S.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Giglio, Louis] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Marlier, Miriam E.] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA.
RP Chen, Y (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM yang.chen@uci.edu
RI collatz, george/D-5381-2012; Morton, Douglas/D-5044-2012; Chen,
Yang/C-6529-2008;
OI Chen, Yang/0000-0002-0993-7081; Kasibhatla, Prasad/0000-0003-3562-3737
FU NASA [NNX08AF64G, NNX10AT83G]
FX Supported by NASA grants NNX08AF64G and NNX10AT83G. The GFED3 carbon
emissions time series is publicly available at www.globalfiredata.org.
NR 34
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U1 6
U2 54
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 NOV 11
PY 2011
VL 334
IS 6057
BP 787
EP 791
DI 10.1126/science.1209472
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 845US
UT WOS:000296849600041
PM 22076373
ER
PT J
AU Bischoff, C
Brizius, A
Buder, I
Chinone, Y
Cleary, K
Dumoulin, RN
Kusaka, A
Monsalve, R
Naess, SK
Newburgh, LB
Reeves, R
Smith, KM
Wehus, IK
Zuntz, JA
Zwart, JTL
Bronfman, L
Bustos, R
Church, SE
Dickinson, C
Eriksen, HK
Ferreira, PG
Gaier, T
Gundersen, JO
Hasegawa, M
Hazumi, M
Huffenberger, KM
Jones, ME
Kangaslahti, P
Kapner, DJ
Lawrence, CR
Limon, M
May, J
McMahon, JJ
Miller, AD
Nguyen, H
Nixon, GW
Pearson, TJ
Piccirillo, L
Radford, SJE
Readhead, ACS
Richards, JL
Samtleben, D
Seiffert, M
Shepherd, MC
Staggs, ST
Tajima, O
Thompson, KL
Vanderlinde, K
Williamson, R
Winstein, B
AF Bischoff, C.
Brizius, A.
Buder, I.
Chinone, Y.
Cleary, K.
Dumoulin, R. N.
Kusaka, A.
Monsalve, R.
Naess, S. K.
Newburgh, L. B.
Reeves, R.
Smith, K. M.
Wehus, I. K.
Zuntz, J. A.
Zwart, J. T. L.
Bronfman, L.
Bustos, R.
Church, S. E.
Dickinson, C.
Eriksen, H. K.
Ferreira, P. G.
Gaier, T.
Gundersen, J. O.
Hasegawa, M.
Hazumi, M.
Huffenberger, K. M.
Jones, M. E.
Kangaslahti, P.
Kapner, D. J.
Lawrence, C. R.
Limon, M.
May, J.
McMahon, J. J.
Miller, A. D.
Nguyen, H.
Nixon, G. W.
Pearson, T. J.
Piccirillo, L.
Radford, S. J. E.
Readhead, A. C. S.
Richards, J. L.
Samtleben, D.
Seiffert, M.
Shepherd, M. C.
Staggs, S. T.
Tajima, O.
Thompson, K. L.
Vanderlinde, K.
Williamson, R.
Winstein, B.
CA QUIET Collaboration
TI FIRST SEASON QUIET OBSERVATIONS: MEASUREMENTS OF COSMIC MICROWAVE
BACKGROUND POLARIZATION POWER SPECTRA AT 43 GHz IN THE MULTIPOLE RANGE
25 <= l <= 475
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; gravitational
waves; inflation; polarization
ID PROBE WMAP OBSERVATIONS; PERSEUS MOLECULAR-COMPLEX; MAPS; BOOMERANG;
EMISSION; TEMPERATURE; CALIBRATION; COVARIANCE; ANTENNAS; DESIGN
AB The Q/U Imaging ExperimenT (QUIET) employs coherent receivers at 43 GHz and 94 GHz, operating on the Chajnantor plateau in the Atacama Desert in Chile, to measure the anisotropy in the polarization of the cosmic microwave background (CMB). QUIET primarily targets the B modes from primordial gravitational waves. The combination of these frequencies gives sensitivity to foreground contributions from diffuse Galactic synchrotron radiation. Between 2008 October and 2010 December, over 10,000 hr of data were collected, first with the 19 element 43 GHz array (3458 hr) and then with the 90 element 94 GHz array. Each array observes the same four fields, selected for low foregrounds, together covering approximate to 1000 deg(2). This paper reports initial results from the 43 GHz receiver, which has an array sensitivity to CMB fluctuations of 69 mu K root s. The data were extensively studied with a large suite of null tests before the power spectra, determined with two independent pipelines, were examined. Analysis choices, including data selection, were modified until the null tests passed. Cross-correlating maps with different telescope pointings is used to eliminate a bias. This paper reports the EE, BB, and EB power spectra in the multipole range l = 25-475. With the exception of the lowest multipole bin for one of the fields, where a polarized foreground, consistent with Galactic synchrotron radiation, is detected with 3 sigma significance, the E-mode spectrum is consistent with the Lambda CDM model, confirming the only previous detection of the first acoustic peak. The B-mode spectrum is consistent with zero, leading to a measurement of the tensor-to-scalar ratio of r = 0.35(-0.87)(+1.06). The combination of a new time-stream "double-demodulation" technique, side-fed Dragonian optics, natural sky rotation, and frequent boresight rotation leads to the lowest level of systematic contamination in the B-mode power so far reported, below the level of r = 0.1.
C1 [Bischoff, C.; Brizius, A.; Buder, I.; Kusaka, A.; Smith, K. M.; Kapner, D. J.; Tajima, O.; Vanderlinde, K.; Winstein, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brizius, A.; Samtleben, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Chinone, Y.; Hasegawa, M.; Hazumi, M.; Tajima, O.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan.
[Chinone, Y.] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Cleary, K.; Reeves, R.; Pearson, T. J.; Radford, S. J. E.; Readhead, A. C. S.; Richards, J. L.; Shepherd, M. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Dumoulin, R. N.; Newburgh, L. B.; Zwart, J. T. L.; Limon, M.; Miller, A. D.; Williamson, R.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Dumoulin, R. N.; Newburgh, L. B.; Zwart, J. T. L.; Limon, M.; Miller, A. D.; Williamson, R.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Monsalve, R.; Bustos, R.; Gundersen, J. O.; Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Naess, S. K.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Wehus, I. K.] Univ Oslo, Dept Phys, N-0316 Oslo, Norway.
[Zuntz, J. A.; Jones, M. E.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Zuntz, J. A.] Oxford Martin Sch, Oxford OX1 3BD, England.
[Zuntz, J. A.] UCL, Dept Phys & Astron, London WC1E, England.
[Bronfman, L.; Bustos, R.; May, J.] Univ Chile, Dept Astron, Santiago, Chile.
[Bustos, R.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Church, S. E.; Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Church, S. E.; Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Dickinson, C.; Piccirillo, L.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Eriksen, H. K.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway.
[Gaier, T.; Kangaslahti, P.; Lawrence, C. R.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Nguyen, H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Nixon, G. W.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Bischoff, C.; Brizius, A.; Buder, I.; Kusaka, A.; Smith, K. M.; Kapner, D. J.; Tajima, O.; Vanderlinde, K.; Winstein, B.] Univ Chicago, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
RP Bischoff, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 43, Cambridge, MA 02138 USA.
EM akito@kicp.uchicago.edu
RI Bronfman, Leonardo/H-9544-2013; Reeves, Rodrigo/H-2812-2014; Williamson,
Ross/H-1734-2015; Pearson, Timothy/N-2376-2015;
OI Bronfman, Leonardo/0000-0002-9574-8454; Reeves,
Rodrigo/0000-0001-5704-271X; Williamson, Ross/0000-0002-6945-2975;
Limon, Michele/0000-0002-5900-2698; Pearson,
Timothy/0000-0001-5213-6231; Bischoff, Colin/0000-0001-9185-6514; Zwart,
Jonathan/0000-0002-4967-946X
FU NSF [AST-0506648, PHY-0355328, AST-0448909, AST-1010016, PHY-0551142];
KAKENHI [20244041, 20740158, 21111002]; PRODEX [C90284]; KIPAC
Enterprise; Strategic Alliance for the Implementation of New
Technologies (SAINT); Fermilab; Kavli Institute for Cosmological
Physics; University of Chicago; National Aeronautics and Space
Administration; JPL; STFC; ERC IRG; Beecroft Institute of Particle
Astrophysics and Cosmology; Oxford Martin School; Science and Technology
Facilities Council; CONICYT [PFB-06]; ALMA-Conicyt [31080022, 31070015];
Sloan foundation
FX Support for the QUIET instrument and operation comes through the NSF
cooperative agreement AST-0506648. Support was also provided by NSF
awards PHY-0355328, AST-0448909, AST-1010016, and PHY-0551142; KAKENHI
20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise
grant; and by the Strategic Alliance for the Implementation of New
Technologies (SAINT).; Some work was performed on the Joint
Fermilab-KICP Supercomputing Cluster, supported by grants from Fermilab,
the Kavli Institute for Cosmological Physics, and the University of
Chicago. Some work was performed on the Titan Cluster, owned and
maintained by the University of Oslo and NOTUR (the Norwegian High
Performance Computing Consortium), and on the Central Computing System,
owned and operated by the Computing Research Center at KEK. Portions of
this work were performed at the Jet Propulsion Laboratory (JPL) and
California Institute of Technology, operating under a contract with the
National Aeronautics and Space Administration. The Q-band polarimeter
modules were developed using funding from the JPL R&TD program.; C.D.
acknowledges an STFC Advanced Fellowship and an ERC IRG grant under FP7.
P. G. F. and J.A.Z. gratefully acknowledge the support of the Beecroft
Institute of Particle Astrophysics and Cosmology, the Oxford Martin
School, and the Science and Technology Facilities Council. L. B., R. B.,
and J.M. acknowledge support from CONICYT project Basal PFB-06. R. B.
acknowledges support from ALMA-Conicyt 31080022 and 31070015. A. D. M.
acknowledges a Sloan foundation fellowship.; PWV measurements were
provided by the Atacama Pathfinder Experiment (APEX). We thank CONICYT
for granting permission to operate within the Chajnantor Scientific
Preserve in Chile, and ALMA for providing site infrastructure support.
Field operations were based at the Don Esteban facility run by
Astro-Norte. We are particularly indebted to the engineers and
technician who maintained and operated the telescope: Jose Cortes,
Cristobal Jara, Freddy Munoz, and Carlos Verdugo.; In addition, we
acknowledge the following people for their assistance in the instrument
design, construction, commissioning, operation, and in data analysis:
Augusto Gutierrez Aitken, Colin Baines, Phil Bannister, Hannah Barker,
Matthew R. Becker, Alex Blein, Mircea Bogdan, April Campbell, Anushya
Chandra, Sea Moon Cho, Emma Curry, Maire Daly, Richard Davis, Fritz
Dejongh, Joy Didier, Greg Dooley, Hans Eide, Will Grainger, Jonathon
Goh, Peter Hamlington, Takeo Higuchi, Seth Hillbrand, Christian Holler,
Ben Hooberman, Kathryn D. Huff, William Imbriale, Koji Ishidoshiro,
Eiichiro Komatsu, Jostein Kristiansen, Richard Lai, Erik Leitch, Kelly
Lepo, Martha Malin, MarkMcCulloch, Oliver Montes, David Moore, Makoto
Nagai, Ian O'Dwyer, Stephen Osborne, Stephen Padin, Felipe Pedreros,
Ashley Perko, Alan Robinson, Jacklyn Sanders, Dale Sanford, Mary Soria,
Alex Sugarbaker, David Sutton, Matias Vidal, Liza Volkova, Edward
Wollack, Stephanie Xenos, and Mark Zaskowski.
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JI Astrophys. J.
PD NOV 10
PY 2011
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DI 10.1088/0004-637X/741/2/111
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500044
ER
PT J
AU Leake, JE
Linton, MG
Antiochos, SK
AF Leake, James E.
Linton, Mark G.
Antiochos, Spiro K.
TI TESTS OF DYNAMICAL FLUX EMERGENCE AS A MECHANISM FOR CORONAL MASS
EJECTION INITIATION (vol 722, pg 550, 2010)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Leake, James E.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Linton, Mark G.] USN, Res Lab, Washington, DC 20375 USA.
[Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA.
RP Leake, JE (reprint author), George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
EM james.leake.ctr.uk@nrl.navy.mil
RI Antiochos, Spiro/D-4668-2012
OI Antiochos, Spiro/0000-0003-0176-4312
NR 1
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500058
ER
PT J
AU Lidz, A
Furlanetto, SR
Oh, SP
Aguirre, J
Chang, TC
Dore, O
Pritchard, JR
AF Lidz, Adam
Furlanetto, Steven R.
Oh, S. Peng
Aguirre, James
Chang, Tzu-Ching
Dore, Olivier
Pritchard, Jonathan R.
TI INTENSITY MAPPING WITH CARBON MONOXIDE EMISSION LINES AND THE REDSHIFTED
21 cm LINE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: theory; intergalactic medium; large-scale structure of
universe
ID MURCHISON-WIDEFIELD-ARRAY; MOLECULAR GAS; INTERGALACTIC MEDIUM;
STAR-FORMATION; HYDROGEN REIONIZATION; DARK-MATTER; PROBING
REIONIZATION; IONIZING EMISSIVITY; COSMIC EVOLUTION; ALPHA EMITTERS
AB We quantify the prospects for using emission lines from rotational transitions of the CO molecule to perform an "intensity mapping" observation at high redshift during the Epoch of Reionization (EoR). The aim of CO intensity mapping is to observe the combined CO emission from many unresolved galaxies, to measure the spatial fluctuations in this emission, and to use this as a tracer of large-scale structure at very early times in the history of our universe. This measurement would help determine the properties of molecular clouds-the sites of star formation-in the very galaxies that reionize the universe. We further consider the possibility of cross-correlating CO intensity maps with future observations of the redshifted 21 cm line. The cross spectrum is less sensitive to foreground contamination than the auto power spectra, and can therefore help confirm the high-redshift origin of each signal. Furthermore, the cross spectrum measurement would help extract key information about the EoR, especially regarding the size distribution of ionized regions. We discuss uncertainties in predicting the CO signal at high redshift, and discuss strategies for improving these predictions. Under favorable assumptions and feasible specifications for a CO survey mapping the CO(2-1) and CO(1-0) lines, the power spectrum of CO emission fluctuations and its cross spectrum with future 21 cm measurements from the Murchison Widefield Array are detectable at high significance.
C1 [Lidz, Adam; Aguirre, James] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Furlanetto, Steven R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Oh, S. Peng] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Chang, Tzu-Ching] Acad Sinica, IAA, Taipei 115, Taiwan.
[Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dore, Olivier] CALTECH, Pasadena, CA 91125 USA.
[Pritchard, Jonathan R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lidz, A (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
EM alidz@sas.upenn.edu
OI Pritchard, Jonathan/0000-0003-4127-5353
FU David and Lucile Packard Foundation; Alfred P. Sloan Foundation; NASA;
NASA Lunar Science Institute [NNA09DB30A]; NSF [AST 0908480]
FX We thank Matt McQuinn for providing the reionization simulations used in
this analysis and for comments on a draft. We are also grateful to Mark
Krumholz and the anonymous referee for helpful remarks that have
improved this paper. This work was initiated at the summer 2010 Aspen 21
cm cosmology meeting. This meeting and a subsequent meeting at the Keck
Institute for Space Sciences helped fuel this work, and we acknowledge
useful conversations with the participants of these meetings. We are
especially grateful to Judd Bowman as a co-organizer of both of these
meetings. S.R.F. was partially supported by the David and Lucile Packard
Foundation, by the Alfred P. Sloan Foundation, and by NASA through the
LUNAR program. The LUNAR consortium (http://lunar.colorado.edu),
headquartered at the University of Colorado, is funded by the NASA Lunar
Science Institute (via Cooperative Agreement NNA09DB30A) to investigate
concepts for astrophysical observatories on the Moon. S.P.O.
acknowledges NSF grant AST 0908480 for support. 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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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
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PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500003
ER
PT J
AU Mainzer, A
Grav, T
Masiero, J
Hand, E
Bauer, J
Tholen, D
McMillan, RS
Spahr, T
Cutri, RM
Wright, E
Watkins, J
Mo, W
Maleszewski, C
AF Mainzer, A.
Grav, T.
Masiero, J.
Hand, E.
Bauer, J.
Tholen, D.
McMillan, R. S.
Spahr, T.
Cutri, R. M.
Wright, E.
Watkins, J.
Mo, W.
Maleszewski, C.
TI NEOWISE STUDIES OF SPECTROPHOTOMETRICALLY CLASSIFIED ASTEROIDS:
PRELIMINARY RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; minor planets, asteroids: general; surveys
ID NEAR-EARTH ASTEROIDS; THERMAL-MODEL CALIBRATION;
INFRARED-SURVEY-EXPLORER; SPECTROSCOPIC SURVEY; MINOR PLANETS;
POPULATION; RADIOMETRY; PHOTOMETRY; TAXONOMY; OBJECTS
AB The NEOWISE data set offers the opportunity to study the variations in albedo for asteroid classification schemes based on visible and near-infrared observations for a large sample of minor planets. We have determined the albedos for nearly 1900 asteroids classified by the Tholen, Bus, and Bus-DeMeo taxonomic classification schemes. We find that the S-complex spans a broad range of bright albedos, partially overlapping the low albedo C-complex at small sizes. As expected, the X-complex covers a wide range of albedos. The multiwavelength infrared coverage provided by NEOWISE allows determination of the reflectivity at 3.4 and 4.6 mu m relative to the visible albedo. The direct computation of the reflectivity at 3.4 and 4.6 mu m enables a new means of comparing the various taxonomic classes. Although C, B, D, and T asteroids all have similarly low visible albedos, the D and T types can be distinguished from the C and B types by examining their relative reflectance at 3.4 and 4.6 mu m. All of the albedo distributions are strongly affected by selection biases against small, low albedo objects, as all objects selected for taxonomic classification were chosen according to their visible light brightness. Due to these strong selection biases, we are unable to determine whether or not there are correlations between size, albedo, and space weathering. We argue that the current set of classified asteroids makes any such correlations difficult to verify. A sample of taxonomically classified asteroids drawn without significant albedo bias is needed in order to perform such an analysis.
C1 [Mainzer, A.; Masiero, J.; Hand, E.; Bauer, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.; Mo, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bauer, J.; Cutri, R. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Tholen, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[McMillan, R. S.; Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[Wright, E.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA.
[Watkins, J.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
FX This publication makes use of data products from the Widefield Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This publication also makes use of data products from
NEOWISE, which is a project of the Jet Propulsion Laboratory/California
Institute of Technology, funded by the Planetary Science Division of the
National Aeronautics and Space Administration. We gratefully acknowledge
the extraordinary services specific to NEOWISE contributed by the
International Astronomical Union's MPC, operated by the
Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for
Astronomical Telegrams, operated by Harvard University. We thank the
paper's referee, Prof. Richard Binzel, for his helpful contributions. 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.
NR 53
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
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DI 10.1088/0004-637X/741/2/90
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500023
ER
PT J
AU Masiero, JR
Mainzer, AK
Grav, T
Bauer, JM
Cutri, RM
Dailey, J
Eisenhardt, PRM
McMillan, RS
Spahr, TB
Skrutskie, MF
Tholen, D
Walker, RG
Wright, EL
DeBaun, E
Elsbury, D
Gautier, T
Gomillion, S
Wilkins, A
AF Masiero, Joseph R.
Mainzer, A. K.
Grav, T.
Bauer, J. M.
Cutri, R. M.
Dailey, J.
Eisenhardt, P. R. M.
McMillan, R. S.
Spahr, T. B.
Skrutskie, M. F.
Tholen, D.
Walker, R. G.
Wright, E. L.
DeBaun, E.
Elsbury, D.
Gautier, T.
Gomillion, S.
Wilkins, A.
TI MAIN BELT ASTEROIDS WITH WISE/NEOWISE. I. PRELIMINARY ALBEDOS AND
DIAMETERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: general; minor planets, asteroids: general
ID INFRARED-SURVEY-EXPLORER; NEAR-EARTH ASTEROIDS; DIGITAL SKY SURVEY;
THERMAL-MODEL; SIZE DISTRIBUTIONS; SPACE-TELESCOPE; 298 BAPTISTINA; K/T
IMPACTOR; 2 PALLAS; FAMILIES
AB We present initial results from the Wide-field Infrared Survey Explorer (WISE), a four-band all-sky thermal infrared survey that produces data well suited for measuring the physical properties of asteroids, and the NEOWISE enhancement to the WISE mission allowing for detailed study of solar system objects. Using a NEATM thermal model fitting routine, we compute diameters for over 100,000 Main Belt asteroids from their IR thermal flux, with errors better than 10%. We then incorporate literature values of visible measurements (in the form of the H absolute magnitude) to determine albedos. Using these data we investigate the albedo and diameter distributions of the Main Belt. As observed previously, we find a change in the average albedo when comparing the inner, middle, and outer portions of the Main Belt. We also confirm that the albedo distribution of each region is strongly bimodal. We observe groupings of objects with similar albedos in regions of the Main Belt associated with dynamical breakup families. Asteroid families typically show a characteristic albedo for all members, but there are notable exceptions to this. This paper is the first look at the Main Belt asteroids in the WISE data, and only represents the preliminary, observed raw size, and albedo distributions for the populations considered. These distributions are subject to survey biases inherent to the NEOWISE data set and cannot yet be interpreted as describing the true populations; the debiased size and albedo distributions will be the subject of the next paper in this series.
C1 [Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.; Eisenhardt, P. R. M.; DeBaun, E.; Elsbury, D.; Gautier, T.; Gomillion, S.; Wilkins, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bauer, J. M.; Cutri, R. M.; Dailey, J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[Skrutskie, M. F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Tholen, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Walker, R. G.] Monterey Inst Res Astron, Monterey, CA USA.
[Wright, E. L.] UCLA Astron, Los Angeles, CA 90095 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.
[Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Masiero, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Joseph.Masiero@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU NASA; Planetary Science Division of the National Aeronautics and Space
Administration
FX We thank the anonymous referee for the helpful comments and suggestions
that led to the improvement of this manuscript. J.R.M. was supported by
an appointment to the NASA Postdoctoral Program at JPL, administered by
Oak Ridge Associated Universities through a contract with NASA. J.R.M.
thanks M. Delbo and M. Mueller for providing access to their thermal
modeling code which was helpful in early test cases. This publication
makes use of data products from the Wide-field Infrared Survey Explorer,
which is a joint project of the University of California, Los Angeles,
and the Jet Propulsion Laboratory/California Institute of Technology,
funded by the National Aeronautics and Space Administration. This
publication also makes use of data products from NEOWISE, which is a
project of the Jet Propulsion Laboratory/California Institute of
Technology, funded by the Planetary Science Division of the National
Aeronautics and Space Administration. 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
worldwide community of dedicated amateur and professional astronomers
devoted to minor planet follow-up observations. We are deeply grateful
for the outstanding contributions of all members of the WISE and NEOWISE
teams.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
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SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500001
ER
PT J
AU Mathur, S
Hekker, S
Trampedach, R
Ballot, J
Kallinger, T
Buzasi, D
Garcia, RA
Huber, D
Jimenez, A
Mosser, B
Bedding, TR
Elsworth, Y
Regulo, C
Stello, D
Chaplin, WJ
De Ridder, J
Hale, SJ
Kinemuchi, K
Kjeldsen, H
Mullally, F
Thompson, SE
AF Mathur, S.
Hekker, S.
Trampedach, R.
Ballot, J.
Kallinger, T.
Buzasi, D.
Garcia, R. A.
Huber, D.
Jimenez, A.
Mosser, B.
Bedding, T. R.
Elsworth, Y.
Regulo, C.
Stello, D.
Chaplin, W. J.
De Ridder, J.
Hale, S. J.
Kinemuchi, K.
Kjeldsen, H.
Mullally, F.
Thompson, S. E.
TI GRANULATION IN RED GIANTS: OBSERVATIONS BY THE KEPLER MISSION AND
THREE-DIMENSIONAL CONVECTION SIMULATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; stars: late-type
ID SOLAR-LIKE OSCILLATIONS; SPECTRAL-LINE FORMATION; EQUATION-OF-STATE; 1ST
4 MONTHS; SURFACE CONVECTION; HYDRODYNAMICAL SIMULATIONS; STELLAR
MICROVARIABILITY; DYNAMICAL ATMOSPHERE; TURBULENT CONVECTION; STARS
AB The granulation pattern that we observe on the surface of the Sun is due to hot plasma rising to the photosphere where it cools down and descends back into the interior at the edges of granules. This is the visible manifestation of convection taking place in the outer part of the solar convection zone. Because red giants have deeper convection zones than the Sun, we cannot a priori assume that their granulation is a scaled version of solar granulation. Until now, neither observations nor one-dimensional analytical convection models could put constraints on granulation in red giants. With asteroseismology, this study can now be performed. We analyze similar to 1000 red giants that have been observed by Kepler during 13 months. We fit the power spectra with Harvey-like profiles to retrieve the characteristics of the granulation (timescale tau(gran) and power P(gran)). We search for a correlation between these parameters and the global acoustic-mode parameter (the position of maximum power, v(max)) as well as with stellar parameters (mass, radius, surface gravity (log g), and effective temperature (T(eff))). We show that tau(eff) alpha v(max)(-0.89) and P(gran) alpha v(max)(-1.90) which is consistent with the theoretical predictions. We find that the granulation timescales of stars that belong to the red clump have similar values while the timescales of stars in the red giant branch are spread in a wider range. Finally, we show that realistic three-dimensional simulations of the surface convection in stars, spanning the (T(eff), log g) range of our sample of red giants, match the Kepler observations well in terms of trends.
C1 [Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Hekker, S.; Elsworth, Y.; Chaplin, W. J.; Hale, S. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Trampedach, R.] Univ Colorado, JILA, Boulder, CO 80309 USA.
[Trampedach, R.] Natl Inst Stand & Technol, Boulder, CO 80309 USA.
[Ballot, J.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Ballot, J.] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
[Kallinger, T.] Univ Vienna, IfA, A-1180 Vienna, Austria.
[Kallinger, T.; De Ridder, J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Buzasi, D.] Eureka Sci, Oakland, CA 94602 USA.
[Garcia, R. A.] CEA DSM CNRS Univ Paris Diderot IRFU SAp, Lab AIM, F-91191 Gif Sur Yvette, France.
[Huber, D.; Bedding, T. R.; Stello, D.] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Jimenez, A.; Regulo, C.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain.
[Jimenez, A.; Regulo, C.] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Mosser, B.] Univ Paris 07, Univ Paris 06, LESIA, UMR8109, F-92195 Meudon, France.
[Kinemuchi, K.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Kjeldsen, H.] Univ Aarhus, Dept Phys & Astron, Danish AsteroSeismol Ctr, DK-8000 Aarhus C, Denmark.
[Mullally, F.; Thompson, S. E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Mathur, S (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA.
RI Ballot, Jerome/G-1019-2010; Hale, Steven/E-3472-2015;
OI Hale, Steven/0000-0002-6402-8382; Kallinger, Thomas/0000-0003-3627-2561;
Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661;
Garcia, Rafael/0000-0002-8854-3776
FU NASAs Science Mission Directorate; National Science Foundation;
Netherlands Organisation for Scientific Research (NWO); Spanish National
Research Plan [AYA2010-17803]; NASA [NNX08AI57G]
FX The authors gratefully acknowledge the Kepler Science Team and all those
who have contributed to making the Kepler mission possible. Funding for
the Kepler Discovery mission is provided by NASAs Science Mission
Directorate. NCAR is supported by the National Science Foundation. S.H.
acknowledges financial support from the Netherlands Organisation for
Scientific Research (NWO). This research was supported by grant
AYA2010-17803 from the Spanish National Research Plan. R.T. was
supported by NASA grant NNX08AI57G.
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SN 0004-637X
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JI Astrophys. J.
PD NOV 10
PY 2011
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DI 10.1088/0004-637X/741/2/119
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500052
ER
PT J
AU Teets, WK
Weintraub, DA
Grosso, N
Principe, D
Kastner, JH
Hamaguchi, K
Richmond, M
AF Teets, William K.
Weintraub, David A.
Grosso, Nicolas
Principe, David
Kastner, Joel H.
Hamaguchi, Kenji
Richmond, Michael
TI X-RAY PRODUCTION BY V1647 Ori DURING OPTICAL OUTBURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation; stars: individual (V1647 Ori); stars: pre-main
sequence; X-rays: stars
ID ILLUMINATING MCNEIL-NEBULA; YOUNG STELLAR OBJECTS; STAR TW HYDRAE; FU
ORIONIS; INFRARED PROPERTIES; IRAS 05436-0007; LINE EMISSION;
XMM-NEWTON; EX LUPI; ACCRETION
AB The pre-main-sequence (PMS) star V1647 Ori has recently undergone two optical/near-infrared (OIR) outbursts that are associated with dramatic enhancements in the stellar accretion rate. Our intensive X-ray monitoring of this object affords the opportunity to investigate whether and how the intense X-ray emission is related to PMS accretion activity. Our analysis of all 14 Chandra X-Ray Observatory observations of V1647 Ori demonstrates that variations in the X-ray luminosity of V1647 Ori are correlated with similar changes in the OIR brightness of this source during both (2003-2005 and 2008) eruptions, strongly supporting the hypothesis that accretion is the primary generation mechanism for the X-ray outbursts. Furthermore, the Chandra monitoring demonstrates that the X-ray spectral properties of the second eruption were strikingly similar to those of the 2003 eruption. We find that X-ray spectra obtained immediately following the second outburst-during which V1647 Ori exhibited high X-ray luminosities, high hardness ratios, and strong X-ray variability-are well modeled as a heavily absorbed (N-H similar to 4 x 10(22) cm(-2)), single-component plasma with characteristic temperatures (kT(X) similar to 2-6 keV) that are consistently too high to be generated via accretion shocks but are in the range expected for plasma heated by magnetic reconnection events. We also find that the X-ray absorbing column has not changed significantly throughout the observing campaign. Since the OIR and X-ray changes are correlated, we hypothesize that these reconnection events either occur in the accretion stream connecting the circumstellar disk to the star or in accretion-enhanced protostellar coronal activity.
C1 [Teets, William K.; Weintraub, David A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Grosso, Nicolas] Univ Strasbourg, CNRS, Observ Astron Strasbourg, UMR 7550, F-67000 Strasbourg, France.
[Principe, David; Kastner, Joel H.; Richmond, Michael] Rochester Inst Technol, Rochester, NY 14623 USA.
[Hamaguchi, Kenji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Teets, WK (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
FU Chandra X-ray Observatory Center [GO8-9016X, GO9-0006X]; NASA
[NAS8-03060]
FX We thank Nuria Calvet for providing early access to the data in Chandra
ObsIDs 10763 and 8585. This research was supported via award numbers
GO8-9016X and GO9-0006X to Vanderbilt University issued by the Chandra
X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA under contract
NAS8-03060.
NR 54
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U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
VL 741
IS 2
AR 83
DI 10.1088/0004-637X/741/2/83
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500016
ER
PT J
AU Williams, BJ
Blair, WP
Blondin, JM
Borkowski, KJ
Ghavamian, P
Long, KS
Raymond, JC
Reynolds, SP
Rho, J
Winkler, PF
AF Williams, Brian J.
Blair, William P.
Blondin, John M.
Borkowski, Kazimierz J.
Ghavamian, Parviz
Long, Knox S.
Raymond, John C.
Reynolds, Stephen P.
Rho, Jeonghee
Winkler, P. Frank
TI RCW 86: A TYPE Ia SUPERNOVA IN A WIND-BLOWN BUBBLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; dust, extinction; ISM: supernova remnants
ID LARGE-MAGELLANIC-CLOUD; X-RAY SPECTROSCOPY; HIGH-RESOLUTION
SPECTROSCOPY; BALMER-DOMINATED SHOCKS; SPITZER-SPACE-TELESCOPE; DUST
DESTRUCTION; REMNANT RCW-86; CYGNUS LOOP; NONRADIATIVE SHOCK; SUZAKU
OBSERVATION
AB We report results from a multi-wavelength analysis of the Galactic supernova remnant RCW 86, the proposed remnant of the supernova of 185 A. D. We show new infrared observations from the Spitzer Space Telescope and the Wide-Field Infrared Survey Explorer, where the entire shell is detected at 24 and 22 mu m. We fit the infrared flux ratios with models of collisionally heated ambient dust, finding post-shock gas densities in the non-radiative shocks of 2.4 and 2.0 cm(-3) in the southwest (SW) and northwest (NW) portions of the remnant, respectively. The Balmer-dominated shocks around the periphery of the shell, large amount of iron in the X-ray-emitting ejecta, and lack of a compact remnant support a Type Ia origin for this remnant. From hydrodynamic simulations, the observed characteristics of RCW 86 are successfully reproduced by an off-center explosion in a low-density cavity carved by the progenitor system. This would make RCW 86 the first known case of a Type Ia supernova in a wind-blown bubble. The fast shocks (>3000 km s(-1)) observed in the northeast are propagating in the low-density bubble, where the shock is just beginning to encounter the shell, while the slower shocks elsewhere have already encountered the bubble wall. The diffuse nature of the synchrotron emission in the SW and NW is due to electrons that were accelerated early in the lifetime of the remnant, when the shock was still in the bubble. Electrons in a bubble could produce gamma rays by inverse-Compton scattering. The wind-blown bubble scenario requires a single-degenerate progenitor, which should leave behind a companion star.
C1 [Williams, Brian J.; Blondin, John M.; Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ghavamian, Parviz; Long, Knox S.] STScI, Baltimore, MD 21218 USA.
[Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rho, Jeonghee] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
RP Williams, BJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
EM bjwilli2@ncsu.edu
FU JPL RSA [1378047]; NSF [AST-0708224]; NASA [NNX11AB14G]; NASA
FX We acknowledge support from Spitzer Guest Observer Grants JPL RSA
1378047, NSF Theory Grant AST-0708224, and NASA Astrophysics Data and
Analysis Program Grant NNX11AB14G. This work is based (in part) on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA. This research has made use of software provided by
the Chandra X-ray Center (CXC) in the application package CIAO. Support
for this work was provided by NASA through an award issued by
JPL/Caltech.
NR 81
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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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
VL 741
IS 2
AR 96
DI 10.1088/0004-637X/741/2/96
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500029
ER
PT J
AU Wood, MA
Still, MD
Howell, SB
Cannizzo, JK
Smale, AP
AF Wood, Matt A.
Still, Martin D.
Howell, Steve B.
Cannizzo, John K.
Smale, Alan P.
TI V344 LYRAE: A TOUCHSTONE SU UMa CATACLYSMIC VARIABLE IN THE KEPLER FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE hydrodynamics; novae, cataclysmic variables; stars: dwarf novae; stars:
individual (V344 Lyr); white dwarfs
ID AM-CANUM-VENATICORUM; X-RAY BINARY; PARTICLE HYDRODYNAMICS SIMULATIONS;
ER-URSAE-MAJORIS; DWARF NOVA; ACCRETION DISKS; CVN STARS; NUMERICAL
SIMULATIONS; NEGATIVE SUPERHUMPS; PERIOD VARIATIONS
AB We report on the analysis of the Kepler short-cadence (SC) light curve of V344 Lyr obtained during 2009 June 20 through 2010 March 19 (Q2-Q4). The system is an SU UMa star showing dwarf nova (DN) outbursts and superoutbursts, and promises to be a touchstone for CV studies for the foreseeable future. The system displays both positive and negative superhumps with periods of 2.20 and 2.06 hr, respectively, and we identify an orbital period of 2.11 hr. The positive superhumps have a maximum amplitude of similar to 0.25 mag, the negative superhumps have a maximum amplitude of similar to 0.8 mag, and the orbital period at quiescence has an amplitude of similar to 0.025 mag. The quality of the Kepler data is such that we can test vigorously the models for accretion disk dynamics that have been emerging in the past several years. The SC data for V344 Lyr are consistent with the model that two physical sources yield positive superhumps: early in the superoutburst, the superhump signal is generated by viscous dissipation within the periodically flexing disk, but late in the superoutburst, the signal is generated as the accretion stream bright spot sweeps around the rim of the non-axisymmetric disk. The disk superhumps are roughly anti-phased with the stream/late superhumps. The V344 Lyr data also reveal negative superhumps arising from accretion onto a tilted disk precessing in the retrograde direction and suggest that negative superhumps may appear during the decline of DN outbursts. The period of negative superhumps has a positive P. in between outbursts.
C1 [Wood, Matt A.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Still, Martin D.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94095 USA.
[Still, Martin D.] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
[Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Cannizzo, John K.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Cannizzo, John K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Cannizzo, John K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RP Wood, MA (reprint author), Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
EM wood@fit.edu
OI Wood, Matthew/0000-0003-0372-9553
FU NASA, Science Mission Directorate; NASA [NAS5-26555]; NASA Office of
Space Science [NAG5-7584]; American Astronomical Society
FX Kepler was selected as the 10th mission of the Discovery Program.
Funding for this mission is provided by NASA, Science Mission
Directorate. All of the data presented in this paper were obtained from
the Multimission Archive at the Space Telescope Science Institute
(MAST). STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for
MAST for non-HST data is provided by the NASA Office of Space Science
via grant NAG5-7584 and by other grants and contracts. This research was
supported in part by the American Astronomical Society's Small Research
Grant Program in the form of page charges. We thank Marcus Hohlmann from
the Florida Institute of Technology and the Domestic Nuclear Detection
Office in the Department of Homeland Security for making computing
resources on a Linux cluster available for this work. We thank Joseph
Patterson of Columbia University for sending us the data used in Figure
19 in electronic form.
NR 89
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
VL 741
IS 2
AR 105
DI 10.1088/0004-637X/741/2/105
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500038
ER
PT J
AU Bradford, CM
Bolatto, AD
Maloney, PR
Aguirre, JE
Bock, JJ
Glenn, J
Kamenetzky, J
Lupu, R
Matsuhara, H
Murphy, EJ
Naylor, BJ
Nguyen, HT
Scott, K
Zmuidzinas, J
AF Bradford, C. M.
Bolatto, A. D.
Maloney, P. R.
Aguirre, J. E.
Bock, J. J.
Glenn, J.
Kamenetzky, J.
Lupu, R.
Matsuhara, H.
Murphy, E. J.
Naylor, B. J.
Nguyen, H. T.
Scott, K.
Zmuidzinas, J.
TI THE WATER VAPOR SPECTRUM OF APM 08279+5255: X-RAY HEATING AND INFRARED
PUMPING OVER HUNDREDS OF PARSECS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; instrumentation: spectrographs; ISM: molecules;
quasars: emission lines
ID WARM MOLECULAR GAS; PHYSICAL PROCESSES; STAR-FORMATION; LINE EMISSION;
HIGH-REDSHIFT; MARKARIAN 231; HOST GALAXY; QUASAR; EXCITATION; Z=3.9
AB We present the rest-frame 200-320 mu m spectrum of the z = 3.91 quasar APM 08279+5255, obtained with Z-Spec at the Caltech Submillimeter Observatory. In addition to the J = 8 -> 7 to J = 13 -> 12 CO rotational transitions which dominate the CO cooling, we find six transitions of water originating at energy levels ranging up to 643 K. Most are first detections at high redshift, and we have confirmed one transition with CARMA. The CO cooling is well described by our X-ray dominated region (XDR) model, assuming L1-100 keV similar to 1 x 10(46) erg s(-1), and that the gas is distributed over a 550-pc size scale, as per the now-favored mu = 4 lensing model. The total observed cooling in water corresponds to 6.5 x 10(9) L-circle dot, comparable to that of CO. We compare the water spectrum with that of Mrk 231, finding that the intensity ratios among the high-lying lines are similar, but with a total luminosity scaled up by a factor of similar to 50. Using this scaling, we estimate an average water abundance relative to H-2 of 1.4 x 10(-7), a good match to the prediction of the chemical network in the XDR model. As with Mrk 231, the high-lying water transitions are excited radiatively via absorption in the rest-frame far-infrared, and we show that the powerful dust continuum in APM 08279+5255 is more than sufficient to pump this massive reservoir of warm water vapor.
C1 [Bradford, C. M.; Bock, J. J.; Naylor, B. J.; Nguyen, H. T.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bradford, C. M.; Bock, J. J.; Naylor, B. J.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
[Bolatto, A. D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Maloney, P. R.; Aguirre, J. E.; Glenn, J.; Kamenetzky, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA.
[Aguirre, J. E.; Lupu, R.; Scott, K.] Univ Penn, Dept Phys, Philadelphia, PA 19104 USA.
[Matsuhara, H.] Japan Aerosp & Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
RP Bradford, CM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Lupu, Roxana/P-9060-2014
OI Lupu, Roxana/0000-0003-3444-5908
FU NASA SARA [NAGS-11911, NAGS-12788]; NSF AST [0807990]; NSF
[AST-0239270]; Research Corporation [RI0928]; Caltech Millikan and JPL
Director's fellowships; NRAO; NASA GSRP; NSF GSRP; National Aeronautics
and Space Administration
FX We are indebted to the staff of the Caltech Submillimeter Observatory
for their help in Z-Spec's commissioning and observing. We acknowledge
the following grants and fellowships: NASA SARA grants NAGS-11911 and
NAGS-12788, NSF AST grant 0807990, an NSF Career grant (AST-0239270) and
a Research Corporation Award (RI0928) to J. Glenn, a Caltech Millikan
and JPL Director's fellowships to C. M. B., an NRAO Jansky fellowship to
J. E. Aguirre, NASA GSRP fellowship to L. Earle, and an NSF GSRP award
to J. Kamenetzky. The research described in this Letter, carried out at
the Jet Propulsion Laboratory, California Institute of Technology, was
done under a contract with the National Aeronautics and Space
Administration.
NR 30
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U1 0
U2 13
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 NOV 10
PY 2011
VL 741
IS 2
AR L37
DI 10.1088/2041-8205/741/2/L37
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844ND
UT WOS:000296753100013
ER
PT J
AU Cours, T
Burgalat, J
Rannou, P
Rodriguez, S
Brahic, A
West, RA
AF Cours, T.
Burgalat, J.
Rannou, P.
Rodriguez, S.
Brahic, A.
West, R. A.
TI DUAL ORIGIN OF AEROSOLS IN TITAN'S DETACHED HAZE LAYER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual
(Titan); radiative transfer; scattering
ID VERTICAL-DISTRIBUTION; AGGREGATE PARTICLES; OPTICAL-PROPERTIES;
ATMOSPHERE; MODEL; BRIGHTNESS; MESOSPHERE; SCATTERING; GROWTH; IMAGES
AB We have analyzed scattered light profiles from the Cassini Imaging Science Subsystem, taken at the limb and at several large phase angles. We also used results from an occultation observed by Ultraviolet Imaging Spectrograph in the ultraviolet. We found that particles responsible for the scattering in the detached haze have an effective radius around 0.15 mu m and the aerosol size distribution follows a power law (exponent about -4.5). We discuss these results along with microphysical constraints and thermal equilibrium of the detached haze, and we conclude that only a strong interaction with atmospheric dynamics can explain such a structure.
C1 [Cours, T.; Burgalat, J.; Rannou, P.] Univ Reims, CNRS, UMR 6089, GSMA, F-51687 Reims 2, France.
[Rannou, P.] Univ Versailles St Quentin, CNRS, UMR 8190, Lab Atmospheres Milieux Observat Spatiales LATMOS, Versailles, France.
[Rodriguez, S.; Brahic, A.] Univ Paris 07, CNRS, UMR 7158, CEA Saclay DSM IRFU SAp,Lab AIM, F-91191 Gif Sur Yvette, France.
[West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cours, T (reprint author), Univ Reims, CNRS, UMR 6089, GSMA, F-51687 Reims 2, France.
EM thibaud.cours@univ-reims.fr
RI RANNOU, Pascal/I-9059-2012; Rodriguez, Sebastien/H-5902-2016
OI Rodriguez, Sebastien/0000-0003-1219-0641
NR 36
TC 6
Z9 6
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 10
PY 2011
VL 741
IS 2
AR L32
DI 10.1088/2041-8205/741/2/L32
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844ND
UT WOS:000296753100008
ER
PT J
AU Yoonessi, M
Heinz, H
Dang, TD
Bai, ZW
AF Yoonessi, Mitra
Heinz, Hendrik
Dang, Thuy D.
Bai, Zongwu
TI Morphology of sulfonated polyarylenethioethersulfone random copolymer
series as proton exchange fuel cells membranes by small angle neutron
scattering
SO POLYMER
LA English
DT Article
DE Fuel cells membrane; Morphology; Neutron scattering
ID PERFLUORINATED IONOMER MEMBRANES; CLASSICAL STATISTICAL MECHANICS;
NAFION MEMBRANES; WATER; MICROEMULSIONS; NANOSTRUCTURE; TRANSPORT;
SWOLLEN; SANS
AB Sulfonated polyarylenethioethersulfone (SPTES) copolymers with high proton conductivity (100-215 mS/cm at 65 degrees C, 85% relative humidity) are promising potential proton exchange membrane (PEM) for fuel cells. Small angle neutron scattering (SANS) of the hydrated SPTES copolymer membranes at 25 degrees C exhibit a nanostructure which can be approximated by correlated polydisperse spherical aggregates containing water molecules with liquid-like ordering (Percus Yevick approximation) and large scale water pockets. The ionic domain radius and the volume packing density of the aggregates present in the hydrated SPTES copolymer membranes at 25 degrees C increased with increasing degree of sulfonation. SPTES-80 with highest degree of sulfonation (71.6%) showed a Guinier plateau at the very low q range (q < 1 x 10(-4) 1/angstrom) indicating presence of isolated large scale morphology (R(g) = 1.3 +/- 0.18 micron). The radius of spherical ionic aggregates present in the hydrated SPTES-50 and SPTES-60 copolymer membranes increased with increasing temperature to 55 degrees C, but the large scale morphology changed to a fractal network. Further increase of the sulfonation degree to 63.3% and 71.6% (SPTES-70 and SPTES-80) resulted in a substantial morphology change of the spherical aggregates to an irregular bicontinuous hydrophobic/hydrophilic morphology for the hydrated SPTES-70 and SPTES-80 copolymer membranes at 55 degrees C. Presence of ionic maxima followed by a power law decay of -4 for SPTES-70 and SPTES-80 copolymer membranes was attributed to the bicontinuous phase morphology at high degree of sulfonation and elevated temperature (55 degrees C). The disruption of the larger scale fractal morphology was characterized by significant decrease in the intermediate scattering intensity. Hydrophobic and hydrophilic domains were separated distinctly by sulfonic groups at the interface showing as power law decay of -4 for all hydrated SPTES copolymers. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Yoonessi, Mitra] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Yoonessi, Mitra] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Heinz, Hendrik] Univ Akron, Dept Polymer Engn, Akron, OH 44325 USA.
[Dang, Thuy D.] USAF, Res Lab, AFRL RXBN, Wright Patterson AFB, OH 45433 USA.
[Bai, Zongwu] Univ Dayton, Res Inst, Dayton, OH 45469 USA.
RP Yoonessi, M (reprint author), Ohio Aerosp Inst, Cleveland, OH 44135 USA.
EM mitra.yoonessi@nasa.gov
RI Heinz, Hendrik/E-3866-2010
OI Heinz, Hendrik/0000-0002-6776-7404
FU Air Force Office of Scientific Research; Materials and Manufacturing
Directorate, Nanostructured and Biological Materials Branch; National
Institute of Standards and Technology [S18-38]; National Science
Foundation [DMR-9986442]
FX The authors would like to thank the Air Force Office of Scientific
Research and Materials and Manufacturing Directorate, Nanostructured and
Biological Materials Branch for funding this research. Richard A. Vaia,
Michael F. Durstock (WPAFB), and Derek Ho (formerly at NIST) are thanked
for the technical discussions support. The National Institute of
Standards and Technology is thanked for funding (Proposal S18-38) to
conduct neutron scattering experiments which were supported by National
Science Foundation under agreement DMR-9986442. The mention of
commercial products does not imply endorsement by NIST, nor does it
imply that the materials or equipment identified are necessarily the
best available for the purpose.
NR 41
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U1 1
U2 26
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0032-3861
J9 POLYMER
JI Polymer
PD NOV 10
PY 2011
VL 52
IS 24
BP 5615
EP 5621
DI 10.1016/j.polymer.2011.09.047
PG 7
WC Polymer Science
SC Polymer Science
GA 846VC
UT WOS:000296930300029
ER
PT J
AU Fioletov, VE
McLinden, CA
Krotkov, N
Moran, MD
Yang, K
AF Fioletov, V. E.
McLinden, C. A.
Krotkov, N.
Moran, M. D.
Yang, K.
TI Estimation of SO2 emissions using OMI retrievals
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OZONE MONITORING INSTRUMENT
AB Satellite sulfur dioxide (SO2) measurements from the Ozone Monitoring Instrument (OMI) satellite sensor, averaged over a period of several years, were compared with emissions inventories for major US sources. Low- and high-spatial frequency filtration was applied to OMI data to reduce the noise and bias to enhance and reveal weak SO2 signals that are otherwise not readily apparent. Averaging a large number of individual observations enables the study of SO2 spatial distributions near larger SO2 emissions sources with an effective resolution superior to that of an individual OMI observation and even to obtain rough estimates of the emissions level from those sources. It is demonstrated that individual sources (or multiple sources within 50 km) with annual SO2 emissions greater than about 70 kT y(-1) produce a statistically significant signal in 3-year averaged OMI data. A correlation of 0.93 was found between OMI SO2 integrated around the source and the annual SO2 emission rate for the sources greater than 70 kT y(-1). OMI SO2 data also indicate a 40% decline in SO2 values over the largest US coal power plants between 2005-2007 and 2008-2010, a value that is consistent with the reported 46% reduction in annual emissions due to the implementation of new SO2 pollution control measures over this period. Citation: Fioletov, V. E., C. A. McLinden, N. Krotkov, M. D. Moran, and K. Yang (2011), Estimation of SO2 emissions using OMI retrievals, Geophys. Res. Lett., 38, L21811, doi:10.1029/2011GL049402.
C1 [Fioletov, V. E.; McLinden, C. A.; Moran, M. D.] Environm Canada, Toronto, ON M3H 5T4, Canada.
[Krotkov, N.; Yang, K.] NASA, Goddard Space Flight Ctr, Astrophys Lab, Greenbelt, MD 20771 USA.
[Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP Fioletov, VE (reprint author), Environm Canada, Toronto, ON M3H 5T4, Canada.
EM vitali.fioletov@ec.gc.ca
RI Krotkov, Nickolay/E-1541-2012;
OI Krotkov, Nickolay/0000-0001-6170-6750; Fioletov,
Vitali/0000-0002-2731-5956
FU NASA Earth Science Division
FX We acknowledge the NASA Earth Science Division for funding of OMI
SO2 product development and analysis. The Dutch-Finnish-built
OMI instrument is part of the NASA EOS Aura satellite payload. The OMI
project is managed by KNMI and the Netherlands Agency for Aero-space
Programs (NIVR). The US Environmental Protection Agency provided
SO2 emissions data. The authors also thank two anonymous
reviewers for their thorough and thoughtful comments.
NR 14
TC 46
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U1 1
U2 29
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 NOV 9
PY 2011
VL 38
AR L21811
DI 10.1029/2011GL049402
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 848BO
UT WOS:000297022100006
ER
PT J
AU Nimmo, F
Bills, BG
Thomas, PC
AF Nimmo, F.
Bills, B. G.
Thomas, P. C.
TI Geophysical implications of the long-wavelength topography of the
Saturnian satellites
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID POLAR TOPOGRAPHY; STEREO IMAGES; GLOBAL SHAPE; PLANETARY; LITHOSPHERE;
ENCELADUS; GANYMEDE; FLEXURE; EUROPA
AB We use limb profiles to quantify the long-wavelength topography of the Saturnian satellites. The degree 2 shapes of Mimas, Enceladus, and Tethys are not consistent with hydrostatic equilibrium. We derive 2-D topographic maps out to spherical harmonic degree 8. There is a good correlation with topography derived from stereo techniques. If uncompensated, topography at degree 3 and higher is large enough to be detectable during close spacecraft flybys. If not properly accounted for, this topography may bias estimates of a satellite's degree 2 gravity coefficients (which are used to determine the moment of inertia). We also derive a one-dimensional variance spectrum (a measure of how roughness varies with wavelength) for each body. The short-wavelength spectral slope is -2 to -2.5, similar to silicate bodies. However, unlike the terrestrial planets, each satellite spectrum shows a reduction in slope at longer wavelengths. If this break in slope is due to a transition from flexural to isostatic support, the globally averaged elastic thickness T(e) of each satellite may be derived. We obtain T(e) values of >= 5 km, 1.5-5 km, approximate to 5 km, and >= 5 km for Tethys, Dione, Rhea, and Iapetus, respectively. For Europa, we obtain T(e) approximate to 1.5 km. These estimates are generally consistent with estimates made using other techniques. For Enceladus, intermediate wavelengths imply T(e) >= 0.5 km, but the variance spectrum at wavelengths greater than 150 km is probably influenced by long-wavelength processes such as convection or shell thickness variations. Impact cratering may also play a role in determining the variance spectra of some bodies.
C1 [Nimmo, F.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Bills, B. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Thomas, P. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Nimmo, F (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
EM fnimmo@es.ucsc.edu
FU UARC; [CDAP-NNX11AK44G]
FX We thank Tony Lowry, an anonymous reviewer, and especially the Editor,
Mark Wieczorek, for insightful comments which improved this manuscript.
Research was supported by CDAP-NNX11AK44G and the UARC.
NR 42
TC 19
Z9 19
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD NOV 9
PY 2011
VL 116
AR E11001
DI 10.1029/2011JE003835
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 848JC
UT WOS:000297046800001
ER
PT J
AU Liu, SG
Bond-Lamberty, B
Hicke, JA
Vargas, R
Zhao, SQ
Chen, J
Edburg, SL
Hu, YM
Liu, JX
McGuire, AD
Xiao, JF
Keane, R
Yuan, WP
Tang, JW
Luo, YQ
Potter, C
Oeding, J
AF Liu, Shuguang
Bond-Lamberty, Ben
Hicke, Jeffrey A.
Vargas, Rodrigo
Zhao, Shuqing
Chen, Jing
Edburg, Steven L.
Hu, Yueming
Liu, Jinxun
McGuire, A. David
Xiao, Jingfeng
Keane, Robert
Yuan, Wenping
Tang, Jianwu
Luo, Yiqi
Potter, Christopher
Oeding, Jennifer
TI Simulating the impacts of disturbances on forest carbon cycling in North
America: Processes, data, models, and challenges
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID NET PRIMARY PRODUCTIVITY; CANADIAN BOREAL FOREST; MOUNTAIN PINE-BEETLE;
BIOME-BGC MODEL; TERRESTRIAL BIOSPHERE MODEL; GLOBAL VEGETATION MODEL;
SOIL ORGANIC-MATTER; LAND-USE HISTORY; CLIMATE-CHANGE; UNITED-STATES
AB Forest disturbances greatly alter the carbon cycle at various spatial and temporal scales. It is critical to understand disturbance regimes and their impacts to better quantify regional and global carbon dynamics. This review of the status and major challenges in representing the impacts of disturbances in modeling the carbon dynamics across North America revealed some major advances and challenges. First, significant advances have been made in representation, scaling, and characterization of disturbances that should be included in regional modeling efforts. Second, there is a need to develop effective and comprehensive process-based procedures and algorithms to quantify the immediate and long-term impacts of disturbances on ecosystem succession, soils, microclimate, and cycles of carbon, water, and nutrients. Third, our capability to simulate the occurrences and severity of disturbances is very limited. Fourth, scaling issues have rarely been addressed in continental scale model applications. It is not fully understood which finer scale processes and properties need to be scaled to coarser spatial and temporal scales. Fifth, there are inadequate databases on disturbances at the continental scale to support the quantification of their effects on the carbon balance in North America. Finally, procedures are needed to quantify the uncertainty of model inputs, model parameters, and model structures, and thus to estimate their impacts on