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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
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; 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; Toffolatti,
   Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner,
   Eduardo/P-7019-2014; 
OI Masi, Silvia/0000-0001-5105-1439; de Bernardis,
   Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; 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;
   Ricciardi, Sara/0000-0002-3807-4043; 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; Lopez-Caniego,
   Marcos/0000-0003-1016-9283; 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;
   Toffolatti, Luigi/0000-0003-2645-7386; Herranz,
   Diego/0000-0003-4540-1417; Zacchei, Andrea/0000-0003-0396-1192; Hivon,
   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.
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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
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   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.
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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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   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
Z9 28
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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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
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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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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.
NR 55
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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 131
EP 157
DI 10.1007/s11207-011-9759-9
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873ER
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.
NR 57
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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 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.
NR 37
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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 345
EP 360
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.
NR 54
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
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JI Sol. Phys.
PD DEC
PY 2011
VL 274
IS 1-2
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EP 425
DI 10.1007/s11207-011-9758-x
PG 27
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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
NR 0
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 1
EP 2
DI 10.1007/s11214-011-9853-1
PG 2
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SC Astronomy & Astrophysics
GA 875AQ
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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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.
PD DEC
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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
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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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JI Space Sci. Rev.
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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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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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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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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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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.
NR 85
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
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.
NR 37
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 487
EP 510
DI 10.1007/s11214-011-9863-z
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
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.
NR 19
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 511
EP 543
DI 10.1007/s11214-011-9855-z
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
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
NR 13
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U1 0
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 545
EP 574
DI 10.1007/s11214-011-9840-6
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
UT WOS:000299002100018
ER

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
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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.
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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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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
TC 46
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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.
NR 226
TC 583
Z9 588
U1 6
U2 39
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 35
DI 10.1088/0067-0049/197/2/35
PG 39
WC Astronomy & Astrophysics
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.
NR 31
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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.
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SC Astronomy & Astrophysics
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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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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.
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SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD DEC
PY 2011
VL 197
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AR 19
DI 10.1088/0067-0049/197/2/19
PG 55
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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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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.
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JI Astrophys. J. Suppl. Ser.
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SC Astronomy & Astrophysics
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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).
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SC Astronomy & Astrophysics
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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).
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Z9 76
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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U1 9
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
TC 32
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U1 1
U2 25
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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U1 4
U2 73
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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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
TC 12
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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
Z9 1
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
TC 2
Z9 2
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
Z9 133
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
Z9 6
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
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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.
NR 24
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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 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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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 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.
NR 35
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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 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.
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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.
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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 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
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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 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.
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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.
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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.
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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 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
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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
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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
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Z9 22
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
TC 5
Z9 5
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
TC 17
Z9 20
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
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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
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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
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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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Z9 7
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
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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
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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
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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
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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
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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
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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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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
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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 115
DI 10.1088/0004-637X/742/2/115
PG 8
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SC Astronomy & Astrophysics
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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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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
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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
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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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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
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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
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SC Astronomy & Astrophysics
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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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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
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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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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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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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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
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
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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
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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
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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
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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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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.
NR 39
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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.
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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
U2 2
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.
C1 [Chary, R. -R.; Chen, X.; Ganga, K.; Huynh, M.; McGehee, P.; Pearson, T. J.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
   [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.
   [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
   [Leonardi, R.; Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
   [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.
   [Dupac, X.; Leonardi, R.; Mendes, L.] Planck Sci Off, ESAC, European Space Agcy, Madrid, Spain.
   [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
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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 CO<INF>2</INF> 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
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U1 3
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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
TC 40
Z9 40
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
TC 2
Z9 2
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
TC 0
Z9 0
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD 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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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 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
TC 17
Z9 17
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
TC 35
Z9 38
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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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
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SC Astronomy & Astrophysics
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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
TC 42
Z9 42
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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U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
VL 742
IS 1
AR 24
DI 10.1088/0004-637X/742/1/24
PG 21
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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.
NR 160
TC 52
Z9 53
U1 0
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD 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.
NR 42
TC 11
Z9 11
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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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JI Astrophys. J.
PD NOV 20
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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.
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J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
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SC Astronomy & Astrophysics
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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.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
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SC Astronomy & Astrophysics
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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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 20
PY 2011
VL 742
IS 1
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DI 10.1088/2041-8205/742/1/L11
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SC Astronomy & Astrophysics
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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.
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SN 2041-8205
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JI Astrophys. J. Lett.
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PY 2011
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IS 1
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SC Astronomy & Astrophysics
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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.
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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 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
TC 178
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 NO<INF>x</INF>
   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
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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
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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
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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
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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
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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
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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
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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
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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
TC 17
Z9 19
U1 7
U2 84
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
NR 31
TC 22
Z9 24
U1 4
U2 22
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 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).
NR 37
TC 66
Z9 66
U1 3
U2 51
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD 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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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).
NR 74
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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 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
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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 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.
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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.
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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 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.
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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
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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
TC 67
Z9 68
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.
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SC Astronomy & Astrophysics
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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
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JI Astrophys. J.
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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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SC Astronomy & Astrophysics
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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.
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JI Astrophys. J.
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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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JI Astrophys. J.
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SC Astronomy & Astrophysics
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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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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
PD NOV 10
PY 2011
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SC Astronomy & Astrophysics
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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.
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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 10
PY 2011
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PG 14
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SC Astronomy & Astrophysics
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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.
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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 10
PY 2011
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SC Astronomy & Astrophysics
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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.
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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 10
PY 2011
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DI 10.1088/0004-637X/741/2/105
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SC Astronomy & Astrophysics
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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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 10
PY 2011
VL 741
IS 2
AR L37
DI 10.1088/2041-8205/741/2/L37
PG 6
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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
TC 12
Z9 12
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
   SO<INF>2</INF> 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
   SO<INF>2</INF> emissions data. The authors also thank two anonymous
   reviewers for their thorough and thoughtful comments.
NR 14
TC 46
Z9 47
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 overall model uncertainty. Working together, the scientific community interested in disturbance and its impacts can identify the most uncertain issues surrounding the role of disturbance in the North American carbon budget and develop working hypotheses to reduce the uncertainty.
C1 [Liu, Shuguang] US Geol Survey, Earth Resources Observat & Sci Ctr, Sioux Falls, SD 57198 USA.
   [Bond-Lamberty, Ben] Joint Global Change Res Inst, DOE Pacific NW Natl Lab, College Pk, MD 20740 USA.
   [Hicke, Jeffrey A.; Edburg, Steven L.] Univ Idaho, Dept Geog, Moscow, ID 83844 USA.
   [Vargas, Rodrigo] Ctr Invest Cient & Educ Super Enseneda, Dept Biol Conservac, Ensenada 22860, Baja California, Mexico.
   [Zhao, Shuqing] Peking Univ, Coll Urban & Environm Sci, Beijing 100871, Peoples R China.
   [Chen, Jing] Univ Toronto, Dept Geog, Toronto, ON M5S 3G3, Canada.
   [Hu, Yueming] S China Agr Univ, Coll Informat, Guangzhou 510642, Guangdong, Peoples R China.
   [Liu, Jinxun; Oeding, Jennifer] Stinger Ghaffarian Technol, Sioux Falls, SD USA.
   [McGuire, A. David] Univ Alaska Fairbanks, Alaska Cooperat Fish & Wildlife Res Unit, US Geol Survey, Fairbanks, AK 99775 USA.
   [Xiao, Jingfeng] Univ New Hampshire, Complex Syst Res Ctr, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
   [Keane, Robert] Rocky Mt Res Stn, Missoula Fire Sci Lab, Missoula, MT 59808 USA.
   [Yuan, Wenping] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
   [Tang, Jianwu] Marine Biol Lab, Ctr Ecosyst, Woods Hole, MA 02543 USA.
   [Luo, Yiqi] Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA.
   [Potter, Christopher] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Liu, SG (reprint author), US Geol Survey, Earth Resources Observat & Sci Ctr, 47914 252nd St, Sioux Falls, SD 57198 USA.
EM sliu@usgs.gov
RI Bond-Lamberty, Ben/C-6058-2008; Hicke, Jeff/M-9677-2013; Tang,
   Jianwu/K-6798-2014; Vargas, Rodrigo/C-4720-2008
OI Bond-Lamberty, Ben/0000-0001-9525-4633; Tang,
   Jianwu/0000-0003-2498-9012; Vargas, Rodrigo/0000-0001-6829-5333
FU U.S. Geological Survey (USGS) in Reston
FX The inception of this synthesis paper was from the North American Carbon
   Program Disturbance Impacts Workshop orchestrated by Eric Kasischke and
   sponsored by the U.S. Geological Survey (USGS) in Reston, 2009. Liu's
   work is supported by USGS Geographic Analysis and Monitoring Program,
   Climate Change R&D Program, and Climate Effects Network Program. Any use
   of trade, firm, or product name is for descriptive purpose only and does
   not imply endorsement by the U.S. Government.
NR 246
TC 54
Z9 56
U1 1
U2 86
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 8
PY 2011
VL 116
AR G00K08
DI 10.1029/2010JG001585
PG 22
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 848SA
UT WOS:000297073200001
ER

PT J
AU Durante, M
   Cucinotta, FA
AF Durante, Marco
   Cucinotta, Francis A.
TI Physical basis of radiation protection in space travel
SO REVIEWS OF MODERN PHYSICS
LA English
DT Article
ID FRAGMENTATION CROSS-SECTIONS; SOLAR PARTICLE EVENTS; GALACTIC
   COSMIC-RAYS; HEAVY-ION BOMBARDMENT; LOW-EARTH-ORBIT; TRACK STRUCTURE;
   CANCER-RISKS; SPECTROMETER AMS-02; MULTIPLE-SCATTERING; HIGH-ENERGY
AB The health risks of space radiation are arguably the most serious challenge to space exploration, possibly preventing these missions due to safety concerns or increasing their costs to amounts beyond what would be acceptable. Radiation in space is substantially different from Earth: high-energy (E) and charge (Z) particles (HZE) provide the main contribution to the equivalent dose in deep space, whereas gamma rays and low-energy alpha particles are major contributors on Earth. This difference causes a high uncertainty on the estimated radiation health risk (including cancer and noncancer effects), and makes protection extremely difficult. In fact, shielding is very difficult in space: the very high energy of the cosmic rays and the severe mass constraints in spaceflight represent a serious hindrance to effective shielding. Here the physical basis of space radiation protection is described, including the most recent achievements in space radiation transport codes and shielding approaches. Although deterministic and Monte Carlo transport codes can now describe well the interaction of cosmic rays with matter, more accurate double-differential nuclear cross sections are needed to improve the codes. Energy deposition in biological molecules and related effects should also be developed to achieve accurate risk models for long-term exploratory missions. Passive shielding can be effective for solar particle events; however, it is limited for galactic cosmic rays (GCR). Active shielding would have to overcome challenging technical hurdles to protect against GCR. Thus, improved risk assessment and genetic and biomedical approaches are a more likely solution to GCR radiation protection issues.
C1 [Durante, Marco] GSI Helmholtzzentrum Schwerionenforsch, Dept Biophys, D-64291 Darmstadt, Germany.
   [Durante, Marco] Tech Univ Darmstadt, Dept Condensed Matter Phys, D-64291 Darmstadt, Germany.
   [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Durante, M (reprint author), GSI Helmholtzzentrum Schwerionenforsch, Dept Biophys, Planckstr 1, D-64291 Darmstadt, Germany.
RI Durante, Marco/K-1315-2014; 
OI Durante, Marco/0000-0002-4615-553X
FU European Space Agency; Beilstein Stiftung; NASA
FX Research on space radiation protection at GSI is partially supported by
   the European Space Agency (IBER contract) and by Beilstein Stiftung
   (NanoBIC contract). Space radiation activities at NASA are supported by
   the NASA Space Radiation Program. We thank Svetlana Ktitareva for
   editing the manuscript, Dr. Myung-Hee Kim for help with figures, and Dr.
   Emanuele Scifoni for useful discussions.
NR 190
TC 87
Z9 89
U1 4
U2 36
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0034-6861
EI 1539-0756
J9 REV MOD PHYS
JI Rev. Mod. Phys.
PD NOV 8
PY 2011
VL 83
IS 4
BP 1245
EP 1281
DI 10.1103/RevModPhys.83.1245
PG 37
WC Physics, Multidisciplinary
SC Physics
GA 850MA
UT WOS:000297197500001
ER

PT J
AU Pegna, R
   Nobili, AM
   Shao, M
   Turyshev, SG
   Catastini, G
   Anselmi, A
   Spero, R
   Doravari, S
   Comandi, GL
   De Michele, A
AF Pegna, R.
   Nobili, A. M.
   Shao, M.
   Turyshev, S. G.
   Catastini, G.
   Anselmi, A.
   Spero, R.
   Doravari, S.
   Comandi, G. L.
   De Michele, A.
TI Abatement of Thermal Noise due to Internal Damping in 2D Oscillators
   with Rapidly Rotating Test Masses
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
AB Mechanical oscillators can be sensitive to very small forces. Low frequency effects are up-converted to higher frequency by rotating the oscillator. We show that for 2-dimensional oscillators rotating at frequency much higher than the signal the thermal noise force due to internal losses and competing with it is abated as the square root of the rotation frequency. We also show that rotation at frequency much higher than the natural one is possible if the oscillator has 2 degrees of freedom, and describe how this property applies also to torsion balances. In addition, in the 2D oscillator the signal is up-converted above resonance without being attenuated as in the 1D case, thus relaxing requirements on the read out. This work indicates that proof masses weakly coupled in 2D and rapidly rotating can play a major role in very small force physics experiments.
C1 [Pegna, R.; Nobili, A. M.; Comandi, G. L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
   [Nobili, A. M.; De Michele, A.] Univ Pisa, Dept Phys E Fermi, I-56127 Pisa, Italy.
   [Shao, M.; Turyshev, S. G.; Spero, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Catastini, G.; Anselmi, A.] Thales Alenia Space Italia, I-10146 Turin, Italy.
RP Pegna, R (reprint author), Ist Nazl Fis Nucl, Sez Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy.
FU ASI (Agenzia Spaziale Italiana); INFN; NASA
FX This work has been supported by ASI (Agenzia Spaziale Italiana) and INFN
   and it was performed in part at JPL, Caltech, under a contract with
   NASA. Thanks are due to the referees.
NR 7
TC 6
Z9 6
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD NOV 7
PY 2011
VL 107
IS 20
AR 200801
DI 10.1103/PhysRevLett.107.200801
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 849MI
UT WOS:000297129200002
PM 22181717
ER

PT J
AU Arridge, CS
   Andre, N
   Khurana, KK
   Russell, CT
   Cowley, SWH
   Provan, G
   Andrews, DJ
   Jackman, CM
   Coates, AJ
   Sittler, EC
   Dougherty, MK
   Young, DT
AF Arridge, C. S.
   Andre, N.
   Khurana, K. K.
   Russell, C. T.
   Cowley, S. W. H.
   Provan, G.
   Andrews, D. J.
   Jackman, C. M.
   Coates, A. J.
   Sittler, E. C.
   Dougherty, M. K.
   Young, D. T.
TI Periodic motion of Saturn's nightside plasma sheet
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ROTATION PERIOD; GALILEO SPACECRAFT; MAGNETOSPHERE; PARTICLE; FIELD
AB Saturn's magnetosphere is replete with magnetospheric periodicities; magnetic fields, plasma parameters, energetic particle fluxes, and radio emissions have all been observed to vary at a period close to that of Saturn's assumed sidereal rotation rate. In particular, periodicities in Saturn's magnetotail can be interpreted in terms of periodic vertical motion of Saturn's outer magnetospheric plasma sheet. The phase relationships between periodicities in different measurable quantities are a key piece of information in validating the various published models that attempt to relate periodicities in different quantities at different locations. It is important to empirically extract these phase relationships from the data in order to distinguish between these models, and to provide further data on which to base new conceptual models. In this paper a simple structural model of the flapping of Saturn's plasma sheet is developed and fitted to plasma densities in the outer magnetosphere, measured by the Cassini electron spectrometer. This model is used to establish the phase relationships between magnetic field periodicities in the cam region of the magnetosphere and the flapping of the plasma sheet. We find that the plasma sheet flaps in phase with B-r and B-theta and in quadrature with the B-phi component in the core/cam region. The plasma sheet phase also has a strong local time asymmetry. These results support some conceptual periodicity models but are in apparent contradiction with others, suggesting that future work is required to either modify the models or study additional phase relationships that are important for these models.
C1 [Arridge, C. S.; Coates, A. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
   [Arridge, C. S.; Jackman, C. M.; Coates, A. J.] UCL Birkbeck, Ctr Planetary Sci, London, England.
   [Andre, N.] CNRS, Inst Rech Astrophys & Planetol, Toulouse, France.
   [Andre, N.] Univ Toulouse, Inst Rech Astrophys & Planetol, UPS OMP, Toulouse, France.
   [Khurana, K. K.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
   [Cowley, S. W. H.; Provan, G.; Andrews, D. J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
   [Jackman, C. M.; Dougherty, M. K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
   [Jackman, C. M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
   [Sittler, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Young, D. T.] SW Res Inst, San Antonio, TX 78238 USA.
RP Arridge, CS (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM csa@mssl.ucl.ac.uk
RI Arridge, Christopher/A-2894-2009; Andrews, David/B-2591-2009; Coates,
   Andrew/C-2396-2008; Russell, Christopher/E-7745-2012; 
OI Arridge, Christopher/0000-0002-0431-6526; Andrews,
   David/0000-0002-7933-0322; Coates, Andrew/0000-0002-6185-3125; Russell,
   Christopher/0000-0003-1639-8298; Jackman, Caitriona/0000-0003-0635-7361
FU STFC; NASA; International Space Science Institute
FX We thank L. K. Gilbert and G. R. Lewis for data processing and software
   support for CAPS at MSSL, and S. Kellock, L. Nani-Alconcel, and P.
   Slootweg at Imperial College for MAG data processing. CSA thanks J. F.
   Carbary, D. E. Jones, M. G. Kivelson, D. G. Mitchell, and D. J.
   Southwood for useful and thought provoking discussions, and K. H.
   Arridge for useful comments on the manuscript. C. S. A. and A. J. C.
   were supported in this work by the STFC rolling grant to MSSL/UCL, C. S.
   A. was also supported by an STFC Postdoctoral fellowship and C. M. J.
   was also supported by the STFC rolling grant to Imperial College. C. T.
   R. and K. K. K. were supported by NASA. S. W. H. C. and G. P. were
   supported by the STFC rolling grant to RSPP/Leicester and D. J. A. by an
   STFC Quota Studentship. C. S. A., N.A., K. K. K., H. J. M., C. T. R.,
   and E. C. S. acknowledge funding and support from the International
   Space Science Institute, where part of this work was discussed. Cassini
   CAPS and MAG operations activities at MSSL and Imperial College were
   supported by STFC.
NR 45
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD NOV 5
PY 2011
VL 116
AR A11205
DI 10.1029/2011JA016827
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 842WH
UT WOS:000296631900004
ER

PT J
AU He, F
   Zhang, XX
   Chen, B
   Fok, MC
AF He, Fei
   Zhang, Xiao-Xin
   Chen, Bo
   Fok, Mei-Ching
TI Reconstruction of the plasmasphere from Moon-based EUV images
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EXTREME-ULTRAVIOLET IMAGER; ELECTRIC-FIELD; INTERPLANETARY GAS; DENSITY;
   PLASMAPAUSE; MODEL; RADIATION; MAGNETOSPHERE; ART; WHISTLER
AB A two-step algorithm for plasmasphere reconstruction from images obtained from the Moon-based extreme ultraviolet (EUV) imager on the Chang'e-3 mission is described and illustrated using simulation data obtained from a dynamic global core plasma model (DGCPM). According to the line of sight (LOS) integration patterns in Moon-based EUV imaging and the outline characteristics of the images, the equatorial plane plasmapause is reconstructed with the Minimum L Algorithm by adopting a magnetic dipole approximation. Having obtained the plasmapause locations, the quasi three-dimensional (3-D) plasmasphere, which is put into the Genetic Algorithm (GA) as an initial guess, is constructed with a statistical model assuming that the density along a field line is a constant. In this way, the plasmaspheric structure and the quasi 3-D plasmaspheric density are extracted from the Moon-based EUV images. This work provides a feasible and applicable method for data analysis of Moon-based EUV imaging, which is to be realized on the Chang'e-3 mission in the Second Phase of Chinese Lunar Exploration Program.
C1 [Zhang, Xiao-Xin] China Meteorol Adm, Natl Ctr Space Weather, Beijing 100081, Peoples R China.
   [He, Fei; Chen, Bo] Chinese Acad Sci, Changchun Inst Opt Fine Mech & Phys, Changchun 130033, Peoples R China.
   [Fok, Mei-Ching] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhang, XX (reprint author), China Meteorol Adm, Natl Ctr Space Weather, 46 Zhongguancun Nandajie, Beijing 100081, Peoples R China.
EM xxzhang@cma.gov.cn
RI he, fei/B-9277-2012; Fok, Mei-Ching/D-1626-2012; 
OI Zhang, XiaoXin/0000-0002-7759-7402
FU National Natural Science Foundation of China [40890160, 10878004,
   40974093]; Major State Basic Research Development Program of China (973
   Program) [2011CB811400]; Special Fund for Public Welfare Industry
   [GYHY200806024]
FX This work is supported by the National Natural Science Foundation of
   China (grants 40890160, 10878004, and 40974093), the Major State Basic
   Research Development Program of China (973 Program) (Grant
   2011CB811400), and the Special Fund for Public Welfare Industry (Grant
   GYHY200806024).
NR 55
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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 5
PY 2011
VL 116
AR A11203
DI 10.1029/2010JA016364
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 842WH
UT WOS:000296631900001
ER

PT J
AU Argus, DF
   Gordon, RG
   DeMets, C
AF Argus, Donald F.
   Gordon, Richard G.
   DeMets, Charles
TI Geologically current motion of 56 plates relative to the no-net-rotation
   reference frame
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE plate motion; reference frame
ID NAZCA-SOUTH-AMERICA; SPACE GEODESY; EULER VECTOR; VELOCITIES; MODEL
AB NNR-MORVEL56, which is a set of angular velocities of 56 plates relative to the unique reference frame in which there is no net rotation of the lithosphere, is determined. The relative angular velocities of 25 plates constitute the MORVEL set of geologically current relative plate angular velocities; the relative angular velocities of the other 31 plates are adapted from Bird (2003). NNR-MORVEL, a set of angular velocities of the 25 MORVEL plates relative to the no-net rotation reference frame, is also determined. Incorporating the 31 plates from Bird (2003), which constitute 2.8% of Earth's surface, changes the angular velocities of the MORVEL plates in the no-net-rotation frame only insignificantly, but provides a more complete description of globally distributed deformation and strain rate. NNR-MORVEL56 differs significantly from, and improves upon, NNR-NUVEL1A, our prior set of angular velocities of the plates relative to the no-net-rotation reference frame, partly due to differences in angular velocity at two essential links of the MORVEL plate circuit, Antarctica-Pacific and Nubia-Antarctica, and partly due to differences in the angular velocities of the Philippine Sea, Nazca, and Cocos plates relative to the Pacific plate. For example, the NNR-MORVEL56 Pacific angular velocity differs from the NNR-NUVEL1A angular velocity by a vector of length 0.039 +/- 0.011 degrees a(-1) (95% confidence limits), resulting in a root-mean-square difference in velocity of 2.8 mm a(-1). All 56 plates in NNR-MORVEL56 move significantly relative to the no-net-rotation reference frame with rotation rates ranging from 0.107 degrees a(-1) to 51.569 degrees a(-1).
C1 [Argus, Donald F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Gordon, Richard G.] Rice Univ, Dept Earth Sci, Houston, TX 77005 USA.
   [DeMets, Charles] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
RP Argus, DF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 238-600, Pasadena, CA 91109 USA.
EM donald.f.argus@jpl.nasa.gov; rgg@rice.edu; chuck@geology.wisc.edu
FU NSF [OCE-0453219, OCE-0527375, OCE-0928961, OCE-1061222]
FX We are grateful to Peter Bird (University of California Los Angeles) for
   the plate boundaries and plate angular velocities in the model of Bird
   [2003]. D. F. Argus completed research at Jet Propulsion Laboratory,
   California Institute of Technology, under contract with the National
   Aeronautics and Space Administration (NASA). RGG was supported by NSF
   grants OCE-0453219, OCE-0527375, OCE-0928961, and OCE-1061222. We thank
   Tim Dixon and an anonymous reviewer for their helpful comments and
   suggestions.
NR 16
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD NOV 5
PY 2011
VL 12
AR Q11001
DI 10.1029/2011GC003751
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 842XE
UT WOS:000296634300001
ER

PT J
AU Shen, ZK
   King, RW
   Agnew, DC
   Wang, M
   Herring, TA
   Dong, D
   Fang, P
AF Shen, Z. -K.
   King, R. W.
   Agnew, D. C.
   Wang, M.
   Herring, T. A.
   Dong, D.
   Fang, P.
TI A unified analysis of crustal motion in Southern California, 1970-2004:
   The SCEC crustal motion map
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID GLOBAL POSITIONING SYSTEM; SAN-ANDREAS-FAULT; WESTERN UNITED-STATES;
   LANDERS EARTHQUAKE SEQUENCE; 1999 HECTOR MINE; SURVEY-MODE GPS; GEODETIC
   MEASUREMENTS; STRAIN ACCUMULATION; POSTSEISMIC DEFORMATION; COSEISMIC
   DISPLACEMENTS
AB To determine crustal motions in and around southern California, we have processed and combined trilateration data collected from 1970 to 1992, VLBI data from 1979 to 1992, and GPS data from 1986 to 2004: a long temporal coverage required in part by the occurrence of several large earthquakes in this region. From a series of solutions for station positions, we have estimated interseismic velocities, coseismic displacements, and postseismic motions. Within the region from 31 N to 38 N. and east to 114 W, the final product includes estimated horizontal velocities for 1009 GPS, 190 trilateration, and 16 VLBI points, with ties between some of these used to stabilize the solution. All motions are relative to the Stable North American Reference Frame (SNARF) as realized through the velocities of 20 GPS stations. This provides a relatively dense set of horizontal velocity estimates, with well-tested errors, for the past quarter century over the plate boundary from 31 N to 36.5 N. These velocities agree well with those from the Plate Boundary Observatory, which apply to a later time period. We also estimated vertical velocities, 533 of which have errors below 2 mm/yr. Most of these velocities are less than 1 mm/yr, but they show 2-4 mm/yr subsidence in the Ventura and Los Angeles basins and in the Salton Trough. Our analysis also included estimates of coseismic and postseismic motions related to the 1992 Landers, 1994 Northridge, 1999 Hector Mine, and 2003 San Simeon earthquakes. Postseismic motions increase logarithmically over time with a time constant of about 10 days, and generally mimic the direction and relative amplitude of the coseismic offsets.
C1 [Shen, Z. -K.; Wang, M.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
   [Agnew, D. C.; Fang, P.] Univ Calif San Diego, Inst Geophys & Planetary Phys, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
   [Dong, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [King, R. W.; Herring, T. A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
   [Shen, Z. -K.] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
RP Shen, ZK (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, 595 Charles E Young Dr, Los Angeles, CA 90095 USA.
EM zshen@ucla.edu; rwk@mit.edu; dagnew@ucsd.edu; mwang@gps.gov.cn;
   tah@mit.edu; danan.dong@jpl.nasa.gov; pfang@ucsd.edu
FU National Science Foundation; US Geological Survey; NASA; USGS
   [G11AP20044]
FX This project depended first and foremost on many efforts to collect
   trilateration data, survey-mode GPS data, and continuous GPS data.
   Trilateration data collection was begun by Jim Savage and Will Prescott;
   we thank them, and Mike Lisowski, for making the data available and
   resolving many issues. For the majority of our sites, the data came from
   survey-mode GPS measurements; we thank all those who organized such
   efforts, the very many observers who collected the data (often under
   trying conditions) and the landowners who provided access. For making
   such data available we especially thank Gerald Bawden (UC Davis), Tim
   Dixon (JPL/University of Miami), Don D'Onofrio (Caltrans), Andrea
   Donnellan (JPL), Javier Gonzalez-Garcia (CICESE), Brad Hager (MIT), Ken
   Hudnut (USGS), Dave Jackson (UCLA), Louise Kellog (UC Davis), Greg
   Lyzenga (Harvey Mudd), Meghan Miller (Central Washington University),
   Frank Monastero and Steve Bjornstad (US Navy Geothermal Program Office),
   William Prescott (USGS), Robert Reilinger (MIT), Jay Satalich
   (Caltrans), Karen Wendt (USGS), and the late Bill Young (Riverside
   County Flood Control). Michael Cline and Mercedes Kim (UCLA) collected a
   considerable volume of data with SCEC funding. We thank David Potter,
   Steve Salyards, and Li-Yu Sung (UCLA) for the initial data assembly. At
   UCSD, Hadley Johnson and Greg Anderson developed and implemented the
   software and procedures for archiving survey-mode data; Don Elliot,
   Heidi Buck, Pam Lehr, and Annika Green accurately decoded and
   transcribed thousands of logsheets. The continuous GPS data from
   southern California and elsewhere made it possible to perform a
   consistent analysis over the long time covered by these observations.
   For his pioneering efforts to establish continuous GPS in southern
   California, for his persistence in maintaining and expanding the
   network, and for his determination to make all the data, local and
   global, readily and reliably available through the SOPAC data center, we
   owe a great deal to the sustained efforts of Yehuda Bock (UCSD). The
   more recent expansion of the SCIGN network also owes much to the efforts
   of many other people, including Ken Hudnut and Will Prescott (USGS),
   Frank Webb (JPL), and John McRaney (USC). Our ability to process data
   over this wide time span owes much to the early development at MIT of
   the GAMIT software by Chuck Counselman, Sergei Gourevitch, Yehuda Bock,
   Rick Abbot, Kurt Feigl, and Mark Murray, and its subsequent improvement
   by Simon McClusky. Processing was made much easier by the analysis done
   at SOPAC, in particular by Rosanne Nikolaidis and Matt van Domselaar. We
   also benefited from the work of Paul Jamason, Michael Scharber, Linette
   Prawirodirdjo, Brent Gilmore, Jeff Dean, and Chris Roelle, in
   maintaining the SOPAC data center (UCSD); SOPAC also provided
   computational resources. In the final step of evaluating the spatial
   consistency of velocities, we benefited greatly through our interaction
   with the fault-modeling work of Rob McCaffrey (Portland State
   University) and Brendan Meade (Harvard). The initial collection of the
   data used here was funded under many grants and programs, notably by the
   National Science Foundation, the US Geological Survey, and NASA. The
   funding for this specific project, and the commitment to making it
   happen, lie with the Southern California Earthquake Center (SCEC) (of
   which this is contribution 1500), under support from the NSF and the
   USGS.; We thank the successive Directors (Kei Aki, Dave Jackson,
   Jean-Bernard Minster, and Tom Jordan) and the rest of the SCEC
   community, for their suppor and patience. Dave Jackson was responsible
   for instigating the idea of the CMM within SCEC, and Ken Hudnut took a
   lead role in the production of Versions 1 and 2 of the CMM. Z.-K. Shen
   acknowledges support from USGS grant G11AP20044.
NR 101
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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 5
PY 2011
VL 116
AR B11402
DI 10.1029/2011JB008549
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 843CA
UT WOS:000296648700001
ER

PT J
AU Vallisneri, M
AF Vallisneri, Michele
TI Beyond the Fisher-Matrix Formalism: Exact Sampling Distributions of the
   Maximum-Likelihood Estimator in Gravitational-Wave Parameter Estimation
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID COALESCING BINARIES; SIGNALS
AB Gravitational-wave astronomers often wish to characterize the expected parameter-estimation accuracy of future observations. The Fisher matrix provides a lower bound on the spread of the maximum-likelihood estimator across noise realizations, as well as the leading-order width of the posterior probability, but it is limited to high signal strengths often not realized in practice. By contrast, Monte Carlo Bayesian inference provides the full posterior for any signal strength, but it is too expensive to repeat for a representative set of noises. Here I describe an efficient semianalytical technique to map the exact sampling distribution of the maximum-likelihood estimator across noise realizations, for any signal strength. This technique can be applied to any estimation problem for signals in additive Gaussian noise.
C1 [Vallisneri, Michele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vallisneri, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU Jet Propulsion Laboratory, California Institute of Technology under
   National Aeronautics and Space Administration
FX I am grateful to G. Cicuta, N. Cornish, C. Cutler, F. Feroz, M. Hobson,
   J. Jewell, I. Mandel, S. Nissanke, E. Onofri, R. O'Shaughnessy, and T.
   Prince, as well as two anonymous referees, for useful suggestions and
   for reviewing this manuscript. This work was supported by the RTD
   program at the Jet Propulsion Laboratory, California Institute of
   Technology, where it was performed under contract with the National
   Aeronautics and Space Administration.
NR 18
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PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD NOV 4
PY 2011
VL 107
IS 19
AR 191104
DI 10.1103/PhysRevLett.107.191104
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 847XG
UT WOS:000297006700002
PM 22181593
ER

PT J
AU Killett, B
   Wahr, J
   Desai, S
   Yuan, D
   Watkins, M
AF Killett, B.
   Wahr, J.
   Desai, S.
   Yuan, D.
   Watkins, M.
TI Arctic Ocean tides from GRACE satellite accelerations
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID CLIMATE EXPERIMENT; GRAVITY RECOVERY; GRAVIMETRY; FIELDS
AB Models are routinely used to remove the effects of global ocean tides from GRACE data during processing to reduce temporal aliasing into monthly GRACE solutions. These models have typically been derived using data from satellite altimeters such as TOPEX/Poseidon. Therefore the Arctic ocean components of tide models are not constrained by altimetry data, potentially resulting in errors that are likely to alias into monthly GRACE gravity fields at all latitudes. Seven years of GRACE inter-satellite accelerations are inverted to solve for corrections to the amplitude and phase of major solar and lunar ocean tides at latitudes north of 50 degrees N using a mascon approach. The tide model originally applied to our data was FES2004, truncated to maximum degree l(max) = 90. Simulations are performed to verify that our inversion algorithm works as designed. Uncertainty estimates are derived from tidal solutions on land, and by subtracting two independent solutions that each use 3.5 years of data. Features above the noise floor in the M-2, K-1, S-2, and O-1 solutions likely represent errors in FES2004. Errors due to truncating the spherical harmonic expansion of FES2004 are too small, and errors in the land mask model (needed to transform sea surface heights into mass) only affect coastal areas and do not produce similar relative amplitudes for any examined tides. In the oceans north of 50 degrees N, these residuals tend to reduce the FES2004 amplitudes for M-2, K-1, S-2, and O-1. Reductions in the variance of accelerations not used in our inversion suggest that our results can be used to improve GRACE processing.
C1 [Killett, B.; Wahr, J.] Univ Colorado Boulder, Dept Phys, Boulder, CO 80309 USA.
   [Killett, B.; Wahr, J.] Univ Colorado Boulder, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
   [Killett, B.; Desai, S.; Yuan, D.; Watkins, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Killett, B (reprint author), Univ Colorado Boulder, Dept Phys, Boulder, CO 80309 USA.
EM bryankillett@gmail.com
FU National Aeronautics and Space Administration (NASA) [NNX08AF026]; JPL
   [1390432]
FX Thanks to the FES2004 authors for their model and sharing the code,
   Wenwen Lu and Sung Byun for providing the GRACE acceleration data,
   Fan-Chi Lin for suggestions that led to the zone of influence algorithm,
   Richard Ray for insight into the origin of the North Pole anomaly in
   K<INF>1</INF>, Sean Swenson for writing the first version of the IDL
   graphics code, and Shin-Chan Han and two anonymous reviewers for helpful
   corrections. This work is supported by NASA grant NNX08AF026 and JPL
   contract 1390432 to the University of Colorado. This work was performed,
   in part, at the Jet Propulsion Laboratory, California Institute of
   Technology, under contract with the National Aeronautics and Space
   Administration. Source code is available at http://bryankillett.com.
NR 36
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U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD NOV 4
PY 2011
VL 116
AR C11005
DI 10.1029/2011JC007111
PG 11
WC Oceanography
SC Oceanography
GA 842SN
UT WOS:000296620600001
ER

PT J
AU Hakkinen, S
   Rhines, PB
   Worthen, DL
AF Haekkinen, Sirpa
   Rhines, Peter B.
   Worthen, Denise L.
TI Atmospheric Blocking and Atlantic Multidecadal Ocean Variability
SO SCIENCE
LA English
DT Article
ID NORTH-ATLANTIC; OSCILLATION; WINTER; HEMISPHERE; TIME
AB Atmospheric blocking over the northern North Atlantic, which involves isolation of large regions of air from the westerly circulation for 5 days or more, influences fundamentally the ocean circulation and upper ocean properties by affecting wind patterns. Winters with clusters of more frequent blocking between Greenland and western Europe correspond to a warmer, more saline subpolar ocean. The correspondence between blocked westerly winds and warm ocean holds in recent decadal episodes (especially 1996 to 2010). It also describes much longer time scale Atlantic multidecadal ocean variability (AMV), including the extreme pre-greenhouse-gas northern warming of the 1930s to 1960s. The space-time structure of the wind forcing associated with a blocked regime leads to weaker ocean gyres and weaker heat exchange, both of which contribute to the warm phase of AMV.
C1 [Haekkinen, Sirpa; Worthen, Denise L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Rhines, Peter B.] Univ Washington, Seattle, WA 98195 USA.
RP Hakkinen, S (reprint author), NASA, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA.
EM sirpa.hakkinen@nasa.gov
RI Hakkinen, Sirpa/E-1461-2012
FU NASA; Ocean Surface Topography (OST) Science Team; NASA through the OST
   Science Team
FX S.H. and D.L.W. were funded by NASA Headquarters Physical Oceanography
   Program and Ocean Surface Topography (OST) Science Team. P. B. R. is
   supported by NASA through the OST Science Team. We thank our reviewers
   for constructive criticism.
NR 27
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PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD NOV 4
PY 2011
VL 334
IS 6056
BP 655
EP 659
DI 10.1126/science.1205683
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 841EG
UT WOS:000296494700051
PM 22053046
ER

PT J
AU Rampino, MR
   Caldeira, K
AF Rampino, Michael R.
   Caldeira, Ken
TI Comment on "Atmospheric PCO2 Perturbations Associated with the Central
   Atlantic Magmatic Province"
SO SCIENCE
LA English
DT Editorial Material
ID CARBON-DIOXIDE; BOUNDARY; METHANE; END
AB Schaller et al. (Research Article, 18 March 2011, p. 1404) proposed that carbon dioxide (CO2) released by the Central Atlantic Magmatic Province eruptions over periods of about 20,000 years led to substantial increases of up to 2000 parts per million (ppm) in the concentration of atmospheric carbon dioxide (Pco(2)) near the Triassic-Jurassic boundary. Use of an atmosphere-ocean model coupled to a carbon-cycle model predicts Pco(2) increases of less than 400 ppm from magmatic volatiles, with only a small climatic impact.
C1 [Rampino, Michael R.] NYU, Dept Biol, New York, NY 10003 USA.
   [Rampino, Michael R.] NYU, Environm Studies Program, New York, NY 10003 USA.
   [Rampino, Michael R.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Caldeira, Ken] Carnegie Inst, Dept Global Ecol, Stanford, CA 94305 USA.
RP Rampino, MR (reprint author), NYU, Dept Biol, 100 Washington Sq E, New York, NY 10003 USA.
EM mrr1@nyu.edu
RI Caldeira, Ken/E-7914-2011
NR 11
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U1 1
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PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD NOV 4
PY 2011
VL 334
IS 6056
DI 10.1126/science.1208653
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 841EG
UT WOS:000296494700029
PM 22053029
ER

PT J
AU Sadleir, JE
   Smith, SJ
   Robinson, IK
   Finkbeiner, FM
   Chervenak, JA
   Bandler, SR
   Eckart, ME
   Kilbourne, CA
AF Sadleir, John E.
   Smith, Stephen J.
   Robinson, Ian K.
   Finkbeiner, Fred M.
   Chervenak, James A.
   Bandler, Simon R.
   Eckart, Megan E.
   Kilbourne, Caroline A.
TI Proximity effects and nonequilibrium superconductivity in
   transition-edge sensors
SO PHYSICAL REVIEW B
LA English
DT Article
ID X-RAY MICROCALORIMETERS; TO-NORMAL TRANSITION; JOSEPHSON-JUNCTIONS;
   CURRENT-DENSITY; NOISE; SPECTROSCOPY; RELAXATION; IMBALANCE; BILAYERS;
   METAL
AB We have recently shown that normal-metal/superconductor (N/S) bilayer superconducting transition-edge sensors (TESs) exhibit weak-link behavior.(1) Here, we extend our understanding to include TESs with added noise-mitigating normal-metal structures (N structures). We find that TESs with added Au structures also exhibit weak-link behavior as evidenced by the exponential temperature dependence of the critical current and Josephson-like oscillations of the critical current with applied magnetic field. We explain our results in terms of an effect converse to the longitudinal proximity effect (LoPE),(1) the lateral inverse proximity effect (LaiPE), for which the order parameter in the N/S bilayer is reduced due to the neighboring N structures. Resistance and critical current measurements are presented as a function of temperature and magnetic field taken on square Mo/Au bilayer TESs with lengths ranging from 8 to 130 mu m with and without added N structures. We observe the inverse proximity effect on the bilayer over in-plane distances many tens of microns and find the transition shifts to lower temperatures scale approximately as the inverse square of the in-plane N-structure separation distance, without appreciable broadening of the transition width. We also present evidence for nonequilbrium superconductivity and estimate a quasiparticle lifetime of 1.8 x 10(-10) s for the bilayer. The LoPE model is also used to explain the increased conductivity at temperatures above the bilayer's steep resistive transition.
C1 [Sadleir, John E.; Robinson, Ian K.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
   [Sadleir, John E.; Smith, Stephen J.; Finkbeiner, Fred M.; Chervenak, James A.; Bandler, Simon R.; Eckart, Megan E.; Kilbourne, Caroline A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Smith, Stephen J.; Eckart, Megan E.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
   [Robinson, Ian K.] UCL, London Ctr Nanotechnol, London WC1E 6BT, England.
   [Bandler, Simon R.] Univ Maryland, College Pk, MD 20742 USA.
   [Bandler, Simon R.] CRESST, College Pk, MD 20742 USA.
RP Sadleir, JE (reprint author), Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
EM john.e.sadleir@nasa.gov
RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010
OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106
NR 51
TC 28
Z9 28
U1 4
U2 26
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-0121
J9 PHYS REV B
JI Phys. Rev. B
PD NOV 3
PY 2011
VL 84
IS 18
AR 184502
DI 10.1103/PhysRevB.84.184502
PG 9
WC Physics, Condensed Matter
SC Physics
GA 845XW
UT WOS:000296861800005
ER

PT J
AU Hu, XM
   Zhang, FQ
   Yu, G
   Fuentes, JD
   Wu, LT
AF Hu, Xiao-Ming
   Zhang, Fuqing
   Yu, Guo
   Fuentes, Jose D.
   Wu, Longtao
TI Contribution of mixed-phase boundary layer clouds to the termination of
   ozone depletion events in the Arctic
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID STRATUS CLOUDS; POLAR SUNRISE; ANNUAL CYCLE; SURFACE; MODEL; TURBULENCE;
   RADIATION; SNOW; MICROPHYSICS; SIMULATIONS
AB During the springtime, ozone depletion events (ODEs) are frequently observed in the Arctic boundary layer. While the chemical reactions associated with the ODEs are understood, the processes responsible for their termination remain unclear. Previous studies proposed that wind shear above the Arctic boundary layer promotes enough vertical mixing to transport ozone-richer air from aloft to the nearly ozone-devoid surface and thus terminates the ODEs. In addition, ozone-richer air masses from mid-latitude regions can migrate to the high Arctic and replenish the Arctic boundary layer with ozone. In the present study, a new mechanism related to mixed-phase boundary layer clouds is proposed as a key contributor to the termination of the ODEs. A single-layer stratocumulus cloud observed over Barrow, Alaska (AK) on April 8, 2008 and its effect on the ODEs is simulated using high-resolution WRF/Chem model. One key finding of this investigation is that the cloud-top radiative cooling can induce strong downdrafts and updrafts. These downdrafts associated with mixed-phase boundary layer clouds can transport ozone-richer air from aloft to the surface, heralding the termination of ODEs. Citation: Hu, X.-M., F. Zhang, G. Yu, J. D. Fuentes, and L. Wu (2011), Contribution of mixed-phase boundary layer clouds to the termination of ozone depletion events in the Arctic, Geophys. Res. Lett., 38, L21801, doi:10.1029/2011GL049229.
C1 [Hu, Xiao-Ming; Zhang, Fuqing; Yu, Guo; Fuentes, Jose D.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
   [Hu, Xiao-Ming] Univ Oklahoma, Ctr Anal & Predict Storms, Norman, OK 73072 USA.
   [Wu, Longtao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hu, XM (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
EM xhu@ou.edu
RI Wu, Longtao/G-5509-2012; Zhang, Fuqing/E-6522-2010; Hu,
   Xiao-Ming/D-8085-2011
OI Zhang, Fuqing/0000-0003-4860-9985; Hu, Xiao-Ming/0000-0002-0769-5090
FU Office of Biological and Environmental Research of the U.S. Department
   of Energy [DE-FG02-05ER64058]; National Aeronautics and Space
   Administration; National Science Foundation [ATM 239012]
FX Guo Yu was supported by the Office of Biological and Environmental
   Research of the U.S. Department of Energy grant DE-FG02-05ER64058 as
   part of the Atmospheric System Research Program. Part of the research
   was carried out at the Jet Propulsion Laboratory, California Institute
   of Technology, under a contract with the National Aeronautics and Space
   Administration. JDF acknowledges support from the National Science
   Foundation to participate in this research (award ATM 239012). The
   authors thank two anonymous reviewers for their assistance in evaluating
   this paper.
NR 29
TC 3
Z9 3
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 3
PY 2011
VL 38
AR L21801
DI 10.1029/2011GL049229
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 842SB
UT WOS:000296619200002
ER

PT J
AU Fisher, R
   Knowlton, N
   Brainard, RE
   Caley, MJ
AF Fisher, Rebecca
   Knowlton, Nancy
   Brainard, Russell E.
   Caley, M. Julian
TI Differences among Major Taxa in the Extent of Ecological Knowledge
   across Four Major Ecosystems
SO PLOS ONE
LA English
DT Article
ID CORAL-REEF ECOSYSTEMS; MARINE ECOSYSTEMS; SPECIES RICHNESS; SEAGRASS
   MEADOWS; BIODIVERSITY; RESILIENCE; DIVERSITY; FUTURE; ASSEMBLAGES;
   MANAGEMENT
AB Existing knowledge shapes our understanding of ecosystems and is critical for ecosystem-based management of the world's natural resources. Typically this knowledge is biased among taxa, with some taxa far better studied than others, but the extent of this bias is poorly known. In conjunction with the publically available World Registry of Marine Species database (WoRMS) and one of the world's premier electronic scientific literature databases (Web of Science (R)), a text mining approach is used to examine the distribution of existing ecological knowledge among taxa in coral reef, mangrove, seagrass and kelp bed ecosystems. We found that for each of these ecosystems, most research has been limited to a few groups of organisms. While this bias clearly reflects the perceived importance of some taxa as commercially or ecologically valuable, the relative lack of research of other taxonomic groups highlights the problem that some key taxa and associated ecosystem processes they affect may be poorly understood or completely ignored. The approach outlined here could be applied to any type of ecosystem for analyzing previous research effort and identifying knowledge gaps in order to improve ecosystem-based conservation and management.
C1 [Fisher, Rebecca] Australian Inst Marine Sci, UWA Oceans Inst, Crawley, WA, Australia.
   [Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
   [Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
   [Brainard, Russell E.] Natl Marine Fisheries Serv, Coral Reef Ecosyst Div, Pacific Isl Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, Honolulu, HI USA.
   [Caley, M. Julian] Australian Inst Marine Sci, Townsville, Qld 4810, Australia.
RP Fisher, R (reprint author), Australian Inst Marine Sci, UWA Oceans Inst, Crawley, WA, Australia.
EM r.fisher@aims.gov.au
OI Fisher, Rebecca/0000-0001-5148-6731
FU BHP Billiton through CReefs Australia
FX This work was funded by BHP Billiton through CReefs Australia, a
   partnership between BHP Billiton, the Great Barrier Reef Foundation, the
   Census of Marine Life and the Australian Institute of Marine Science
   (AIMS). CReefs Australia is a node of the Census of Coral Reef
   Ecosystems (CReefs), a project of the Census of Marine Life. The funders
   had no role in study design, data collection and analysis, decision to
   publish, or preparation of the manuscript.
NR 48
TC 6
Z9 6
U1 2
U2 24
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD NOV 2
PY 2011
VL 6
IS 11
AR e26556
DI 10.1371/journal.pone.0026556
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 849WB
UT WOS:000297154900024
PM 22073172
ER

PT J
AU Harris, S
   Veraverbeke, S
   Hook, S
AF Harris, Sarah
   Veraverbeke, Sander
   Hook, Simon
TI Evaluating Spectral Indices for Assessing Fire Severity in Chaparral
   Ecosystems (Southern California) Using MODIS/ASTER (MASTER) Airborne
   Simulator Data
SO REMOTE SENSING
LA English
DT Article
DE fire severity; burn severity; Normalized Burn Ratio; emissivity; surface
   temperature; southern California; chaparral; MASTER
ID NORMALIZED BURN RATIO; 2007 PELOPONNESE WILDFIRES; ADJUSTED VEGETATION
   INDEX; LANDSAT THEMATIC MAPPER; BOREAL FOREST; AFRICAN SAVANNAS;
   TIME-SERIES; IMAGES; INTENSITY; REGIMES
AB Wildland fires are a yearly recurring phenomenon in many terrestrial ecosystems. Accurate fire severity estimates are of paramount importance for modeling fire-induced trace gas emissions and rehabilitating post-fire landscapes. We used high spatial and high spectral resolution MODIS/ASTER (MASTER) airborne simulator data acquired over four 2007 southern California burns to evaluate the effectiveness of 19 different spectral indices, including the widely used Normalized Burn Ratio (NBR), for assessing fire severity in southern California chaparral. Ordinal logistic regression was used to assess the goodness-of-fit between the spectral index values and ordinal field data of severity. The NBR and three indices in which the NBR is enhanced with surface temperature or emissivity data revealed the best performance. Our findings support the operational use of the NBR in chaparral ecosystems by Burned Area Emergency Rehabilitation (BAER) projects, and demonstrate the potential of combining optical and thermal data for assessing fire severity. Additional testing in more burns, other ecoregions and different vegetation types is required to fully understand how (thermally enhanced) spectral indices relate to fire severity.
C1 [Harris, Sarah] Monash Univ, Sch Geog & Environm Sci, Melbourne, Vic 3800, Australia.
   [Harris, Sarah; Veraverbeke, Sander; Hook, Simon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Veraverbeke, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sarah.harris@monash.edu; Sander.S.Veraverbeke@jpl.nasa.gov;
   Simon.J.Hook@jpl.nasa.gov
RI Veraverbeke, Sander/H-2301-2012
OI Veraverbeke, Sander/0000-0003-1362-5125
FU National Aeronautics and Space Administration
FX The research described in this paper was carried out at the Jet
   Propulsion Laboratory (JPL), California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration. The
   authors would like to thank Marti Witter and Tim Handley of the National
   Park Service of the Santa Monica Mountains National Recreation Area, and
   Lorri Peltz-Lewis of the Department of Interior, US Bureau of
   Reclamation for supplying field data. The JPL authors' copyright for
   this publication is held by the California Institute of Technology. The
   authors would like to thank the anonymous reviewers for their
   constructive remarks.
NR 76
TC 13
Z9 13
U1 2
U2 13
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD NOV
PY 2011
VL 3
IS 11
BP 2403
EP 2419
DI 10.3390/rs3112403
PG 17
WC Remote Sensing
SC Remote Sensing
GA 978OX
UT WOS:000306754600006
ER

PT J
AU Yoo, JM
   Won, YI
   Cho, YJ
   Jeong, MJ
   Shin, DB
   Lee, SJ
   Lee, YR
   Oh, SM
   Ban, SJ
AF Yoo, Jung-Moon
   Won, Young-In
   Cho, Young-Jun
   Jeong, Myeong-Jae
   Shin, Dong-Bin
   Lee, Suk-Jo
   Lee, Yu-Ri
   Oh, Soo-Min
   Ban, Soo-Jin
TI Temperature Trends in the Skin/Surface, Mid-troposphere and Low
   Stratosphere Near Korea from Satellite and Ground Measurements
SO ASIA-PACIFIC JOURNAL OF ATMOSPHERIC SCIENCES
LA English
DT Article
DE Temperature trend; AIRS/AMSU; MODIS; Korea; AWS; RAOB; arctic
   oscillation
ID LAND-SURFACE TEMPERATURE; ARCTIC OSCILLATION; SOUTHERN OSCILLATION;
   SOLAR-CYCLE; VALIDATION; WINTER; ENSO; SEA; ICE; QBO
AB Various types of satellite (AIRS/AMSU, MODIS) and ground measurements are used to analyze temperature trends in the four vertical layers (skin/surface, mid-troposphere, and low stratosphere) around the Korean Peninsula (123-132 degrees E, 33-44 degrees N) during the period from September 2002 to August 2010. The ground-based observations include 72 Surface Meteorological Stations (SMSs), 6 radiosonde stations (RAOBs), 457 Automatic Weather Stations (AWSs) over the land, and 5 buoy stations over the ocean. A strong warming (0.052 K yr(-1)) at the surface, and a weak warming (0.004 similar to 0.010 K yr(-1)) in the mid-troposphere and low stratosphere have been found from satellite data, leading to an unstable atmospheric layer. The AIRS/AMSU warming trend over the ocean surface around the Korean Peninsula is about 2.5 times greater than that over the land surface. The ground measurements from both SMS and AWS over the land surface of South Korea also show a warming of 0.043 similar to 0.082 K yr(-1), consistent with the satellite observations. The correlation average (r = 0.80) between MODIS skin temperature and ground measurement is significant. The correlations between AMSU and RAOB are very high (0.91 similar to 0.95) in the anomaly time series, calculated from the spatial averages of monthly mean temperature values. However, the warming found in the AMSU data is stronger than that from the RAOB at the surface. The opposite feature is present above the mid-troposphere, indicating that there is a systematic difference. Warming phenomena (0.012 similar to 0.078 K yr(-1)) are observed from all three data sets (SMS, AWS, MODIS), which have been corroborated by the coincident measurements at five ground stations. However, it should also be noted that the observed trends are subject to large uncertainty as the corresponding 95% confidence intervals tend to be larger than the observed signals due to large thermal variability and the relatively short periods of the satellite-based temperature records. The EOF analysis of monthly mean temperature anomalies indicates that the tropospheric temperature variability near Korea is primarily linked to the Arctic Oscillation (AO), and secondarily to ENSO (El Nino and Southern Oscillation). However, the low stratospheric temperature variability is mainly associated with Southern Oscillation and then additionally with Quasi-Biennial Oscillation (QBO). Uncertainties from the different spatial resolutions between satellite data are discussed in the trends.
C1 [Yoo, Jung-Moon; Lee, Yu-Ri; Oh, Soo-Min] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
   [Won, Young-In] NASA GSFC, Wyle IS, Greenbelt, MD USA.
   [Cho, Young-Jun; Shin, Dong-Bin] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
   [Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Dept Atmospher & Environm Sci, Kangnung, South Korea.
   [Lee, Suk-Jo; Ban, Soo-Jin] Natl Inst Environm Res, Inchon, South Korea.
RP Yoo, JM (reprint author), Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
EM yjm@ewha.ac.kr
FU National Research Foundation of Korea (NRF); Korea government (MEST)
   [2010-0001905]
FX This work was supported by the National Research Foundation of Korea
   (NRF) grant funded by Korea government (MEST) (No. 2010-0001905). We
   would like to thank Goddard Earth Sciences Data Information and Services
   Center (GES DISC) for providing AIRS/AMSU-A data. We are also grateful
   to NASA Land Process Distributed Active Archive Center (LP DAAC) for
   providing MODIS LST data. We appreciate Korea Meteorological
   Administration (KMA) meteorological resources division for the
   ground-based temperature data.
NR 49
TC 5
Z9 5
U1 0
U2 4
PU KOREAN METEOROLOGICAL SOC
PI SEOUL
PA SHINKIL-DONG 508, SIWON BLDG 704, YONGDUNGPO-GU, SEOUL, 150-050, SOUTH
   KOREA
SN 1976-7633
J9 ASIA-PAC J ATMOS SCI
JI Asia-Pac. J. Atmos. Sci.
PD NOV
PY 2011
VL 47
IS 5
BP 439
EP 455
DI 10.1007/s13143-011-0029-4
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 919RH
UT WOS:000302345800004
ER

PT J
AU Galeazzi, M
   Chiao, M
   Collier, MR
   Cravens, T
   Koutroumpa, D
   Kuntz, KD
   Lepri, S
   McCammon, D
   Porter, FS
   Prasai, K
   Robertson, I
   Snowden, S
   Uprety, Y
AF Galeazzi, Massimiliano
   Chiao, Meng
   Collier, Michael R.
   Cravens, Thomas
   Koutroumpa, Dimitra
   Kuntz, Kip D.
   Lepri, Susan
   McCammon, Dan
   Porter, Frederick S.
   Prasai, Krishna
   Robertson, Ina
   Snowden, Steve
   Uprety, Youaraj
TI DXL: a sounding rocket mission for the study of solar wind charge
   exchange and local hot bubble X-ray emission
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE X-ray; Solar wind charge exchange; Local hot bubble; Diffuse X-ray
   background
ID XMM-NEWTON OBSERVATIONS; INTERGALACTIC MEDIUM; BACKGROUND FLUX; ROSAT
   SURVEY; SUZAKU; FIELD; GAS; MAGNETOSHEATH; HELIOSPHERE; ENVIRONMENT
AB The Diffuse X-rays from the Local galaxy (DXL) mission is an approved sounding rocket project with a first launch scheduled around December 2012. Its goal is to identify and separate the X-ray emission generated by solar wind charge exchange from that of the local hot bubble to improve our understanding of both. With 1,000 cm(2) proportional counters and grasp of about 10 cm(2) sr both in the 1/4 and 3/4 keV bands, DXL will achieve in a 5-min flight what cannot be achieved by current and future X-ray satellites.
C1 [Galeazzi, Massimiliano; Prasai, Krishna; Uprety, Youaraj] Univ Miami, Coral Gables, FL 33124 USA.
   [Chiao, Meng; Collier, Michael R.; Koutroumpa, Dimitra; Porter, Frederick S.; Snowden, Steve] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Cravens, Thomas; Robertson, Ina] Univ Kansas, Lawrence, KS 66045 USA.
   [Kuntz, Kip D.] Johns Hopkins Univ, Baltimore, MD USA.
   [Lepri, Susan] Univ Michigan, Ann Arbor, MI 48109 USA.
   [McCammon, Dan] Univ Wisconsin, Madison, WI USA.
RP Galeazzi, M (reprint author), Univ Miami, Coral Gables, FL 33124 USA.
EM galeazzi@physics.miami.edu
RI Porter, Frederick/D-3501-2012; Snowden, Steven/D-5292-2012; Lepri,
   Susan/I-8611-2012; Collier, Michael/I-4864-2013; Uprety,
   Youaraj/C-8104-2015
OI Porter, Frederick/0000-0002-6374-1119; Collier,
   Michael/0000-0001-9658-6605; Uprety, Youaraj/0000-0001-9101-2063
FU National Aeronautics and Space Administration (NASA) [NNX11AF04G]
FX The investigation is supported by the National Aeronautics and Space
   Administration (NASA), grant # NNX11AF04G. DK acknowledges support from
   a NASA Postdoctoral Program fellowship administered by Oak Ridge
   Associated Universities.
NR 56
TC 9
Z9 9
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD NOV
PY 2011
VL 32
IS 2
BP 83
EP 99
DI 10.1007/s10686-011-9249-y
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 898VE
UT WOS:000300769600001
ER

PT J
AU Hosack, M
   Black, JK
   Deines-Jones, P
   Dennis, BR
   Hill, JE
   Jahoda, K
   Shih, AY
   Urba, CE
   Emslie, AG
AF Hosack, Michael
   Black, J. Kevin
   Deines-Jones, Philip
   Dennis, Brian R.
   Hill, Joanne E.
   Jahoda, Keith
   Shih, Albert Y.
   Urba, Christian E.
   Emslie, A. Gordon
TI Imaging X-ray Polarimeter for Solar Flares (IXPS)
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Solar flare; X-ray polarimetry; Particle tracking; GEM; TPC
ID NEGATIVE-ION DRIFT; 2002 JULY 23; POLARIZATION MEASUREMENTS;
   CRAB-NEBULA; PROPORTIONAL-COUNTERS; RHESSI; BREMSSTRAHLUNG; EMISSION;
   DIRECTIVITY; ELECTRONS
AB We describe the design of a balloon-borne Imaging X-ray Polarimeter for Solar flares (IXPS). This novel instrument, a Time Projection Chamber (TPC) for photoelectric polarimetry, will be capable of measuring polarization at the few percent level in the 20-50 keV energy range during an M-or X-class flare, and will provide imaging information at the similar to 10 arcsec level. The primary objective of such observations is to determine the directivity of nonthermal high-energy electrons producing solar hard X-rays, and hence to learn about the particle acceleration and energy release processes in solar flares. Secondary objectives include the separation of the thermal and nonthermal components of the flare X-ray emissions and the separation of photospheric albedo fluxes from direct emissions.
C1 [Hosack, Michael; Deines-Jones, Philip; Dennis, Brian R.; Hill, Joanne E.; Jahoda, Keith; Shih, Albert Y.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Hosack, Michael] ADNET Syst Inc, Rockville, MD 20852 USA.
   [Black, J. Kevin] Rock Creek Sci, Silver Spring, MD 20910 USA.
   [Hill, Joanne E.; Urba, Christian E.] CRESST Univ Space Res Assoc, Columbia, MD 21044 USA.
   [Emslie, A. Gordon] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
RP Hosack, M (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM mghosack@yahoo.com; brian.r.dennis@nasa.gov
RI Dennis, Brian/C-9511-2012; Shih, Albert/D-4714-2012; Jahoda,
   Keith/D-5616-2012
FU NASA
FX This work was supported by NASA through the Heliophysics Low Cost Access
   to Space program of the Research Opportunities in Space and Earth
   Sciences (ROSES). Several individuals have provided technical assistance
   or advice for this project. We thank Bob Baker and Ken Simms for custom
   electronics. Michael Dion assisted especially with the cleaning and
   stretching of GEMs. Jeff Martoff provided useful advice and ideas
   particularly concerning detector gas. Zach Prieskorn's work with a
   similar detector provided a useful baseline for testing and
   troubleshooting various problems. Phil Kaaret suggested polarization
   through Compton scattering and provided references. We thank Toru
   Tamagawa for help communicating with Japanese suppliers. Finally, we
   thank Zhong Zhong for assistance concerning the use of synchrotron
   radiation for 20-50 keV polarized X-rays.
NR 61
TC 2
Z9 2
U1 1
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD NOV
PY 2011
VL 32
IS 2
BP 101
EP 125
DI 10.1007/s10686-011-9254-1
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 898VE
UT WOS:000300769600002
ER

PT J
AU Gronoff, G
   Wedlund, CS
AF Gronoff, Guillaume
   Wedlund, Cyril Simon
TI Auroral Formation and Plasma Interaction Between Magnetized Objects
   Simulated With the Planeterrella
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Glow discharge devices; ionosphere; magnetosphere; planets; plasma
   devices
AB The Planeterrella is a space plasma simulator, based on Kristian Birkeland's historical experiment, the "Terrella." This device not only makes it possible to simulate interactions between an electrode and a magnetized sphere in many different geometries but also to simulate interactions between two magnetized spheres. Such configurations allow the visualization of phenomena unknown to Birkeland, such as an emitting body (Io) immersed in a magnetosphere (Jupiter) or the aurora on the night side of a planet where one magnetic pole points toward the Sun (Uranus).
C1 [Gronoff, Guillaume] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Wedlund, Cyril Simon] BIRA IASB, B-1180 Brussels, Belgium.
RP Gronoff, G (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM guillaume.p.gronoff@nasa.gov; Cyril.Simon@aeronomie.be
OI Gronoff, Guillaume/0000-0002-0331-7076
FU NPP
FX Manuscript received November 30, 2010; revised April 12, 2011; accepted
   April 16, 2011. Date of publication May 23, 2011; date of current
   version November 9, 2011. The work of G. Gronoff was supported by the
   NPP Program.
NR 4
TC 2
Z9 2
U1 4
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD NOV
PY 2011
VL 39
IS 11
SI SI
BP 2712
EP 2713
DI 10.1109/TPS.2011.2147804
PN 1
PG 2
WC Physics, Fluids & Plasmas
SC Physics
GA 884CV
UT WOS:000299683400329
ER

PT J
AU Cruden, BA
AF Cruden, Brett A.
TI Spectrally and Spatially Resolved Radiance Measurement in High-Speed
   Shock Waves for Planetary Entry
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Aerospace simulation; plasma diagnostics; plasma measurements; shock
   waves; spectral analysis; spectroradiometers; spectroscopy
AB Three-dimensional images of absolute radiance as a function of position and wavelength are obtained for shock-heated plasmas traveling in a shock tube at velocities near Mach 30. Vacuum optics coupled to a shock tube are used to image the shock onto four separate spectrometers, which, in turn, disperse the radiation in wavelength onto intensified CCD arrays covering selected spectral ranges from the vacuum ultraviolet (> 120 nm) through midwave infrared (< 5000 nm). Quantitative radiometry performed in this fashion is used to benchmark radiative heating codes used in sizing spacecraft thermal protection systems.
C1 ERC Corp, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Cruden, BA (reprint author), ERC Corp, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Brett.A.Cruden@nasa.gov
FU Orion Multi-Purpose Crew Vehicle (MPCV); NASA Ames Research Center
   [NNA10DE12C]
FX Manuscript received December 1, 2010; revised April 11, 2011; accepted
   April 16, 2011. Date of publication August 30, 2011; date of current
   version November 9, 2011. This work supported by the Orion Multi-Purpose
   Crew Vehicle (MPCV) Aerosciences Project. Work by ERC is carried out
   under contract NNA10DE12C from NASA Ames Research Center.
NR 3
TC 0
Z9 0
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD NOV
PY 2011
VL 39
IS 11
SI SI
BP 2718
EP 2719
DI 10.1109/TPS.2011.2162255
PN 1
PG 2
WC Physics, Fluids & Plasmas
SC Physics
GA 884CV
UT WOS:000299683400332
ER

PT J
AU Weatherford, BR
   Foster, JE
   Kamhawi, H
AF Weatherford, Brandon R.
   Foster, John E.
   Kamhawi, Hani
TI Visible Plume From a Low-Power ECR Waveguide Plasma Cathode for Electric
   Propulsion Systems
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Electron sources; plasma sources; propulsion
AB A waveguide ECR plasma cathode is being investigated as a long-lived alternative to thermionic emitter-based electron sources for ion beam neutralization in electric propulsion systems. The present device can deliver up to 4.2 A of electron current, on argon or xenon, with low power consumption and high gas utilization.
C1 [Weatherford, Brandon R.; Foster, John E.] Univ Michigan, Dept Nucl Engn & Radiol Sci, Ann Arbor, MI 48109 USA.
   [Kamhawi, Hani] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Weatherford, BR (reprint author), Univ Michigan, Dept Nucl Engn & Radiol Sci, Ann Arbor, MI 48109 USA.
EM brweathe@umich.edu; jefoster@umich.edu; hani.kamhawi-1@nasa.gov
FU NASA; Michigan Space Grant Consortium
FX Manuscript received December 1, 2010; revised March 21, 2011; accepted
   March 27, 2011. Date of publication May 12, 2011; date of current
   version November 9, 2011. This work was supported in part by the NASA
   Graduate Student Researchers Program and in part by the Michigan Space
   Grant Consortium Fellowships.
NR 4
TC 0
Z9 0
U1 2
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD NOV
PY 2011
VL 39
IS 11
SI SI
BP 2942
EP 2943
DI 10.1109/TPS.2011.2138722
PN 1
PG 2
WC Physics, Fluids & Plasmas
SC Physics
GA 884CV
UT WOS:000299683400444
ER

PT J
AU Kumar, A
   Done, J
   Dudhia, J
   Niyogi, D
AF Kumar, Anil
   Done, James
   Dudhia, Jimy
   Niyogi, Dev
TI Simulations of Cyclone Sidr in the Bay of Bengal with a high-resolution
   model: sensitivity to large-scale boundary forcing
SO METEOROLOGY AND ATMOSPHERIC PHYSICS
LA English
DT Article
ID TROPICAL CYCLONES; SATELLITE DATA; PREDICTION
AB The predictability of Cyclone Sidr in the Bay of Bengal was explored in terms of track and intensity using the Advanced Research Hurricane Weather Research Forecast (AHW) model. This constitutes the first application of the AHW over an area that lies outside the region of the North Atlantic for which this model was developed and tested. Several experiments were conducted to understand the possible contributing factors that affected Sidr's intensity and track simulation by varying the initial start time and domain size. Results show that Sidr's track was strongly controlled by the synoptic flow at the 500-hPa level, seen especially due to the strong mid-latitude westerly over north-central India. A 96-h forecast produced westerly winds over north-central India at the 500-hPa level that were notably weaker; this likely caused the modeled cyclone track to drift from the observed actual track. Reducing the model domain size reduced model error in the synoptic-scale winds at 500 hPa and produced an improved cyclone track. Specifically, the cyclone track appeared to be sensitive to the upstream synoptic flow, and was, therefore, sensitive to the location of the western boundary of the domain. However, cyclone intensity remained largely unaffected by this synoptic wind error at the 500-hPa level. Comparison of the high resolution, moving nested domain with a single coarser resolution domain showed little difference in tracks, but resulted in significantly different intensities. Experiments on the domain size with regard to the total precipitation simulated by the model showed that precipitation patterns and 10-m surface winds were also different. This was mainly due to the mid-latitude westerly flow across the west side of the model domain. The analysis also suggested that the total precipitation pattern and track was unchanged when the domain was extended toward the east, north, and south. Furthermore, this highlights our conclusion that Sidr was influenced from the west side of the domain. The displacement error was significantly reduced after the domain size from the western model boundary was decreased. Study results demonstrate the capability and need of a high-resolution mesoscale modeling framework for simulating the complex interactions that contribute to the formation of tropical cyclones over the Bay of Bengal region.
C1 [Kumar, Anil; Done, James; Dudhia, Jimy] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
   [Kumar, Anil; Niyogi, Dev] Purdue Univ, W Lafayette, IN 47907 USA.
RP Kumar, A (reprint author), NASA GSFC, Hydrol Sci Branch, Code 614-3, Greenbelt, MD 20771 USA.
EM anil.kumar@nasa.gov
RI Dudhia, Jimy/B-1287-2008
OI Dudhia, Jimy/0000-0002-2394-6232
FU National Science Foundation; NSF CAREER [ATM-0847472]
FX The authors would like to thank Qingnong Xiao from MMM Division at
   National Center for Atmospheric Research (NCAR) for the internal review
   on an initial draft. We also thank NCAR supercomputing resources for
   providing computing GAUS. NCAR is sponsored by the National Science
   Foundation. The study also benefited from the NSF CAREER grant
   (ATM-0847472).
NR 26
TC 11
Z9 11
U1 0
U2 3
PU SPRINGER WIEN
PI WIEN
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA
SN 0177-7971
J9 METEOROL ATMOS PHYS
JI Meteorol. Atmos. Phys.
PD NOV
PY 2011
VL 114
IS 3-4
BP 123
EP 137
DI 10.1007/s00703-011-0161-9
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 887TG
UT WOS:000299952300004
ER

PT J
AU Mao, XL
   Bol'shakov, AA
   Choi, I
   McKay, CP
   Perry, DL
   Sorkhabi, O
   Russo, RE
AF Mao, Xianglei
   Bol'shakov, Alexander A.
   Choi, Inhee
   McKay, Christopher P.
   Perry, Dale L.
   Sorkhabi, Osman
   Russo, Richard E.
TI Laser Ablation Molecular Isotopic Spectrometry: Strontium and its
   isotopes
SO SPECTROCHIMICA ACTA PART B-ATOMIC SPECTROSCOPY
LA English
DT Article
DE Optical isotopic measurement; Laser ablation plasma; Molecular emission
   spectrum; LIBS analysis; LAMIS of strontium
ID INDUCED BREAKDOWN SPECTROSCOPY; ATOMIC EMISSION-SPECTROMETRY; TITANATE
   THIN-FILMS; INDUCED PLASMA; ABUNDANCE RATIOS; SOLID SAMPLES; URANIUM;
   TRANSITION; CHEMISTRY; MARS
AB The experimental details are reported of Laser Ablation Molecular Isotopic Spectrometry (LAMIS) and its application for performing optical isotopic analysis of solid strontium-containing samples in ambient atmospheric air at normal pressure. The LAMIS detection method is described for strontium isotopes from samples of various chemical and isotopic compositions. The results demonstrate spectrally resolved measurements of the three individual Sr-86, Sr-87, and Sr-88 isotopes that are quantified using multivariate calibration of spectra. The observed isotopic shifts are consistent with those calculated theoretically. The measured spectra of diatomic oxide and halides of strontium generated in laser ablation plasmas demonstrate the isotopic resolution and capability of LAMIS. In particular, emission spectra of SrO and SrF molecular radicals provided clean and well resolved spectral signatures for the naturally occurring strontium isotopes. A possibility is discussed of using LAMIS of strontium isotopes for radiogenic age determination. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Mao, Xianglei; Choi, Inhee; Perry, Dale L.; Sorkhabi, Osman; Russo, Richard E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
   [Bol'shakov, Alexander A.; Russo, Richard E.] Appl Spectra Inc, Fremont, CA 94538 USA.
   [McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Russo, RE (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
EM rerusso@lbl.gov
RI Bol'shakov, Alexander/A-9258-2015
OI Bol'shakov, Alexander/0000-0002-6034-7079
FU Defense Threat Reduction Administration (DTRA) of the U. S. Department
   of Defense [LB09005541, LB09005541A]; U.S. Department of Energy through
   the National Nuclear Security Administration (NNSA) [DE-AC02-05CH11231];
   NASA [NNX10CA07C]
FX This work was supported by the Defense Threat Reduction Administration
   (DTRA) of the U. S. Department of Defense under Federal Award Nos.
   LB09005541 and LB09005541A, and Contract No. DE-AC02-05CH11231 awarded
   by the U.S. Department of Energy through the National Nuclear Security
   Administration (NNSA) and NASA Contract No. NNX10CA07C awarded to
   Applied Spectra, Inc.
NR 68
TC 43
Z9 44
U1 1
U2 37
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0584-8547
J9 SPECTROCHIM ACTA B
JI Spectroc. Acta Pt. B-Atom. Spectr.
PD NOV-DEC
PY 2011
VL 66
IS 11-12
BP 767
EP 775
DI 10.1016/j.sab.2011.12.002
PG 9
WC Spectroscopy
SC Spectroscopy
GA 890GE
UT WOS:000300132300001
ER

PT J
AU Birn, J
   Hesse, M
   Zenitani, S
AF Birn, J.
   Hesse, M.
   Zenitani, S.
TI Reconnection in compressible plasmas: Extended conversion region
SO PHYSICS OF PLASMAS
LA English
DT Article
DE magnetic reconnection; plasma magnetohydrodynamics; plasma simulation;
   plasma transport processes
ID CHALLENGE
AB The classical Sweet-Parker approach to steady-state magnetic reconnection is extended into the regime of large resistivity (small magnetic Reynolds or Lundquist number) when the aspect ratio between the outflow and inflow scale, delta = d/L, approaches unity. In a previous paper [Paper I, Hesse , Phys. Plasmas 18, 042104 (2011)], the vicinity of the dissipation site ("diffusion region") was investigated. In this paper, the approach is extended to cover larger sites, in which the energy transfer and conversion is not confined to the diffusion region. Consistent with the results of Paper I, we find that increasing aspect ratio delta is associated with increasing compression, increasing reconnection rate for low beta, but slightly decreasing rate for higher beta, decreasing outflow speed, and increasing outflow magnetic field. These trends are stronger for lower beta. Deviations from the traditional Sweet-Parker limit delta -> 0 become significant for R(m) less than or similar to 10, where R(m) is the magnetic Reynolds number (Lundquist number) based on the half-thickness of the current layer responsible for the Ohmic dissipation. They are also more significant for small gamma, that is, for increasing compressibility. In contrast to the results of Paper I, but consistent with earlier results for delta < 1, we find that in this limit the outflow speed is given by the Alfveacuten speed nu(A) in the inflow region and the energy conversion is given by an even split of Poynting flux into enthalpy flux and bulk kinetic energy flux. However, with increasing delta the conversion to enthalpy flux becomes more and more dominant. (C) 2011 American Institute of Physics. [doi:10.1063/1.3626836]
C1 [Birn, J.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
   [Hesse, M.; Zenitani, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Birn, J (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
EM jbirn@lanl.gov
RI Hesse, Michael/D-2031-2012; Zenitani, Seiji/D-7988-2013; NASA MMS,
   Science Team/J-5393-2013
OI Zenitani, Seiji/0000-0002-0945-1815; NASA MMS, Science
   Team/0000-0002-9504-5214
FU U.S. Department of Energy; NASA
FX This work was performed under the auspices of the U.S. Department of
   Energy, supported by NASA's Supporting Research and Technology Program
   and MMS mission.
NR 12
TC 5
Z9 5
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
   MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD NOV
PY 2011
VL 18
IS 11
AR 111202
DI 10.1063/1.3626836
PG 7
WC Physics, Fluids & Plasmas
SC Physics
GA 860HU
UT WOS:000297940200006
ER

PT J
AU Abbasi, R
   Abdou, Y
   Abu-Zayyad, T
   Ackermann, M
   Adams, J
   Aguilar, JA
   Ahlers, M
   Allen, MM
   Altmann, D
   Andeen, K
   Auffenberg, J
   Bai, X
   Baker, M
   Barwick, SW
   Baum, V
   Bay, R
   Alba, JLB
   Beattie, K
   Beatty, JJ
   Bechet, S
   Becker, JK
   Becker, KH
   Benabderrahmane, ML
   BenZvi, S
   Berdermann, J
   Berghaus, P
   Berley, D
   Bernardini, E
   Bertrand, D
   Besson, DZ
   Bindig, D
   Bissok, M
   Blaufuss, E
   Blumenthal, J
   Boersma, DJ
   Bohm, C
   Bose, D
   Boser, S
   Botner, O
   Brown, AM
   Buitink, S
   Caballero-Mora, KS
   Carson, M
   Chirkin, D
   Christy, B
   Clevermann, F
   Cohen, S
   Colnard, C
   Cowen, DF
   Silva, AHC
   D'Agostino, MV
   Danninger, M
   Daughhetee, J
   Davis, JC
   De Clercq, C
   Degner, T
   Demirors, L
   Descamps, F
   Desiati, P
   de Vries-Uiterweerd, G
   DeYoung, T
   Diaz-Velez, JC
   Dierckxsens, M
   Dreyer, J
   Dumm, JP
   Dunkman, M
   Eisch, J
   Ellsworth, RW
   Engdegard, O
   Euler, S
   Evenson, PA
   Fadiran, O
   Fazely, AR
   Fedynitch, A
   Feintzeig, J
   Feusels, T
   Filimonov, K
   Finley, C
   Fischer-Wasels, T
   Fox, BD
   Franckowiak, A
   Franke, R
   Gaisser, TK
   Gallagher, J
   Gerhardt, L
   Gladstone, L
   Glusenkamp, T
   Goldschmidt, A
   Goodman, JA
   Gora, D
   Grant, D
   Griesel, T
   Gross, A
   Grullon, S
   Gurtner, M
   Ha, C
   Ismail, AH
   Hallgren, A
   Halzen, F
   Han, K
   Hanson, K
   Heinen, D
   Helbing, K
   Hellauer, R
   Hickford, S
   Hill, GC
   Hoffman, KD
   Hoffmann, B
   Homeier, A
   Hoshina, K
   Huelsnitz, W
   Hulss, JP
   Hulth, PO
   Hultqvist, K
   Hussain, S
   Ishihara, A
   Jakobi, E
   Jacobsen, J
   Japaridze, GS
   Johansson, H
   Kampert, KH
   Kappes, A
   Karg, T
   Karle, A
   Kenny, P
   Kiryluk, J
   Kislat, F
   Klein, SR
   Kohne, H
   Kohnen, G
   Kolanoski, H
   Kopke, L
   Kopper, S
   Koskinen, DJ
   Kowalski, M
   Kowarik, T
   Krasberg, M
   Kroll, G
   Kurahashi, N
   Kuwabara, T
   Labare, M
   Laihem, K
   Landsman, H
   Larson, MJ
   Lauer, R
   Lunemann, J
   Madsen, J
   Marotta, A
   Maruyama, R
   Mase, K
   Matis, HS
   Meagher, K
   Merck, M
   Meszaros, P
   Meures, T
   Miarecki, S
   Middell, E
   Milke, N
   Miller, J
   Montaruli, T
   Morse, R
   Movit, SM
   Nahnhauer, R
   Nam, JW
   Naumann, U
   Nygren, DR
   Odrowski, S
   Olivas, A
   Olivo, M
   O'Murchadha, A
   Panknin, S
   Paul, L
   de los Heros, CP
   Petrovic, J
   Piegsa, A
   Pieloth, D
   Porrata, R
   Posselt, J
   Price, PB
   Przybylski, GT
   Rawlins, K
   Redl, P
   Resconi, E
   Rhode, W
   Ribordy, M
   Richard, AS
   Richman, M
   Rodrigues, JP
   Rothmaier, F
   Rott, C
   Ruhe, T
   Rutledge, D
   Ruzybayev, B
   Ryckbosch, D
   Sander, HG
   Santander, M
   Sarkar, S
   Schatto, K
   Schmidt, T
   Schonwald, A
   Schukraft, A
   Schulte, L
   Schultes, A
   Schulz, O
   Schunck, M
   Seckel, D
   Semburg, B
   Seo, SH
   Sestayo, Y
   Seunarine, S
   Silvestri, A
   Singh, K
   Slipak, A
   Spiczak, GM
   Spiering, C
   Stamatikos, M
   Stanev, T
   Stezelberger, T
   Stokstad, RG
   Stossl, A
   Strahler, EA
   Strom, R
   Stuer, M
   Sullivan, GW
   Swillens, Q
   Taavola, H
   Taboada, I
   Tamburro, A
   Tepe, A
   Ter-Antonyan, S
   Tilav, S
   Toale, PA
   Toscano, S
   Tosi, D
   van Eijndhoven, N
   Vandenbroucke, J
   Van Overloop, A
   van Santen, J
   Vehring, M
   Voge, M
   Walck, C
   Waldenmaier, T
   Wallraff, M
   Walter, M
   Weaver, C
   Wendt, C
   Westerhoff, S
   Whitehorn, N
   Wiebe, K
   Wiebusch, CH
   Williams, DR
   Wischnewski, R
   Wissing, H
   Wolf, M
   Wood, TR
   Woschnagg, K
   Xu, C
   Xu, DL
   Xu, XW
   Yanez, JP
   Yodh, G
   Yoshida, S
   Zarzhitsky, P
   Zoll, M
AF Abbasi, R.
   Abdou, Y.
   Abu-Zayyad, T.
   Ackermann, M.
   Adams, J.
   Aguilar, J. A.
   Ahlers, M.
   Allen, M. M.
   Altmann, D.
   Andeen, K.
   Auffenberg, J.
   Bai, X.
   Baker, M.
   Barwick, S. W.
   Baum, V.
   Bay, R.
   Alba, J. L. Bazo
   Beattie, K.
   Beatty, J. J.
   Bechet, S.
   Becker, J. K.
   Becker, K. -H.
   Benabderrahmane, M. L.
   BenZvi, S.
   Berdermann, J.
   Berghaus, P.
   Berley, D.
   Bernardini, E.
   Bertrand, D.
   Besson, D. Z.
   Bindig, D.
   Bissok, M.
   Blaufuss, E.
   Blumenthal, J.
   Boersma, D. J.
   Bohm, C.
   Bose, D.
   Boeser, S.
   Botner, O.
   Brown, A. M.
   Buitink, S.
   Caballero-Mora, K. S.
   Carson, M.
   Chirkin, D.
   Christy, B.
   Clevermann, F.
   Cohen, S.
   Colnard, C.
   Cowen, D. F.
   Silva, A. H. Cruz
   D'Agostino, M. V.
   Danninger, M.
   Daughhetee, J.
   Davis, J. C.
   De Clercq, C.
   Degner, T.
   Demiroers, L.
   Descamps, F.
   Desiati, P.
   de Vries-Uiterweerd, G.
   DeYoung, T.
   Diaz-Velez, J. C.
   Dierckxsens, M.
   Dreyer, J.
   Dumm, J. P.
   Dunkman, M.
   Eisch, J.
   Ellsworth, R. W.
   Engdegard, O.
   Euler, S.
   Evenson, P. A.
   Fadiran, O.
   Fazely, A. R.
   Fedynitch, A.
   Feintzeig, J.
   Feusels, T.
   Filimonov, K.
   Finley, C.
   Fischer-Wasels, T.
   Fox, B. D.
   Franckowiak, A.
   Franke, R.
   Gaisser, T. K.
   Gallagher, J.
   Gerhardt, L.
   Gladstone, L.
   Gluesenkamp, T.
   Goldschmidt, A.
   Goodman, J. A.
   Gora, D.
   Grant, D.
   Griesel, T.
   Gross, A.
   Grullon, S.
   Gurtner, M.
   Ha, C.
   Ismail, A. Haj
   Hallgren, A.
   Halzen, F.
   Han, K.
   Hanson, K.
   Heinen, D.
   Helbing, K.
   Hellauer, R.
   Hickford, S.
   Hill, G. C.
   Hoffman, K. D.
   Hoffmann, B.
   Homeier, A.
   Hoshina, K.
   Huelsnitz, W.
   Huelss, J. -P.
   Hulth, P. O.
   Hultqvist, K.
   Hussain, S.
   Ishihara, A.
   Jakobi, E.
   Jacobsen, J.
   Japaridze, G. S.
   Johansson, H.
   Kampert, K. -H.
   Kappes, A.
   Karg, T.
   Karle, A.
   Kenny, P.
   Kiryluk, J.
   Kislat, F.
   Klein, S. R.
   Koehne, H.
   Kohnen, G.
   Kolanoski, H.
   Koepke, L.
   Kopper, S.
   Koskinen, D. J.
   Kowalski, M.
   Kowarik, T.
   Krasberg, M.
   Kroll, G.
   Kurahashi, N.
   Kuwabara, T.
   Labare, M.
   Laihem, K.
   Landsman, H.
   Larson, M. J.
   Lauer, R.
   Luenemann, J.
   Madsen, J.
   Marotta, A.
   Maruyama, R.
   Mase, K.
   Matis, H. S.
   Meagher, K.
   Merck, M.
   Meszaros, P.
   Meures, T.
   Miarecki, S.
   Middell, E.
   Milke, N.
   Miller, J.
   Montaruli, T.
   Morse, R.
   Movit, S. M.
   Nahnhauer, R.
   Nam, J. W.
   Naumann, U.
   Nygren, D. R.
   Odrowski, S.
   Olivas, A.
   Olivo, M.
   O'Murchadha, A.
   Panknin, S.
   Paul, L.
   Perez de los Heros, C.
   Petrovic, J.
   Piegsa, A.
   Pieloth, D.
   Porrata, R.
   Posselt, J.
   Price, P. B.
   Przybylski, G. T.
   Rawlins, K.
   Redl, P.
   Resconi, E.
   Rhode, W.
   Ribordy, M.
   Richard, A. S.
   Richman, M.
   Rodrigues, J. P.
   Rothmaier, F.
   Rott, C.
   Ruhe, T.
   Rutledge, D.
   Ruzybayev, B.
   Ryckbosch, D.
   Sander, H. -G.
   Santander, M.
   Sarkar, S.
   Schatto, K.
   Schmidt, T.
   Schoenwald, A.
   Schukraft, A.
   Schulte, L.
   Schultes, A.
   Schulz, O.
   Schunck, M.
   Seckel, D.
   Semburg, B.
   Seo, S. H.
   Sestayo, Y.
   Seunarine, S.
   Silvestri, A.
   Singh, K.
   Slipak, A.
   Spiczak, G. M.
   Spiering, C.
   Stamatikos, M.
   Stanev, T.
   Stezelberger, T.
   Stokstad, R. G.
   Stoessl, A.
   Strahler, E. A.
   Strom, R.
   Stueer, M.
   Sullivan, G. W.
   Swillens, Q.
   Taavola, H.
   Taboada, I.
   Tamburro, A.
   Tepe, A.
   Ter-Antonyan, S.
   Tilav, S.
   Toale, P. A.
   Toscano, S.
   Tosi, D.
   van Eijndhoven, N.
   Vandenbroucke, J.
   Van Overloop, A.
   van Santen, J.
   Vehring, M.
   Voge, M.
   Walck, C.
   Waldenmaier, T.
   Wallraff, M.
   Walter, M.
   Weaver, Ch.
   Wendt, C.
   Westerhoff, S.
   Whitehorn, N.
   Wiebe, K.
   Wiebusch, C. H.
   Williams, D. R.
   Wischnewski, R.
   Wissing, H.
   Wolf, M.
   Wood, T. R.
   Woschnagg, K.
   Xu, C.
   Xu, D. L.
   Xu, X. W.
   Yanez, J. P.
   Yodh, G.
   Yoshida, S.
   Zarzhitsky, P.
   Zoll, M.
CA IceCube Collaboration
TI IceCube sensitivity for low-energy neutrinos from nearby supernovae
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE neutrinos; supernovae: general; instrumention: detectors
ID CORE-COLLAPSE SUPERNOVAE; EQUATION-OF-STATE; EXPLOSION MECHANISM;
   GRAVITATIONAL-WAVE; NEUTRON-STAR; DETECTOR; BURST; SN1987A; SIGNAL;
   WATER
AB This paper describes the response of the IceCube neutrino telescope located at the geographic south pole to outbursts of MeV neutrinos from the core collapse of nearby massive stars. IceCube was completed in December 2010 forming a lattice of 5160 photomultiplier tubes that monitor a volume of similar to 1 km(3) in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater than 100 GeV. Owing to subfreezing ice temperatures, the photomultiplier dark noise rates are particularly low. Hence IceCube can also detect large numbers of MeV neutrinos by observing a collective rise in all photomultiplier rates on top of the dark noise. With 2 ms timing resolution, IceCube can detect subtle features in the temporal development of the supernova neutrino burst. For a supernova at the galactic center, its sensitivity matches that of a background-free megaton-scale supernova search experiment. The sensitivity decreases to 20 standard deviations at the galactic edge (30 kpc) and 6 standard deviations at the Large Magellanic Cloud (50 kpc). IceCube is sending triggers from potential supernovae to the Supernova Early Warning System. The sensitivity to neutrino properties such as the neutrino hierarchy is discussed, as well as the possibility to detect the neutronization burst, a short outbreak of nu(e)'s released by electron capture on protons soon after collapse. Tantalizing signatures, such as the formation of a quark star or a black hole as well as the characteristics of shock waves, are investigated to illustrate IceCube's capability for supernova detection.
C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
   [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subat & Radiat Phys, B-9000 Ghent, Belgium.
   [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
   [Adams, J.; Brown, A. M.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
   [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
   [Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
   [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
   [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
   [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Miarecki, S.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Ackermann, M.; Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Silva, A. H. Cruz; Danninger, M.; Franke, R.; Gora, D.; Jakobi, E.; Kislat, F.; Lauer, R.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
   [Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
   [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
   [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
   [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
   [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium.
   [Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
   [Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
   [Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
   [Altmann, D.; Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Gluesenkamp, T.; Heinen, D.; Hoffmann, B.; Huelss, J. -P.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
   [Bohm, C.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden.
   [Bohm, C.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
   [Bose, D.; De Clercq, C.; Labare, M.; Singh, K.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
   [Boeser, S.; Degner, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Stueer, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
   [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; Perez de los Heros, C.; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
   [Clevermann, F.; Koehne, H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
   [Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
   [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
   [Allen, M. M.; Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Larson, M. J.; Meszaros, P.; Rutledge, D.; Slipak, A.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
   [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
   [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
   [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
   [Fazely, A. R.; Richard, A. S.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
   [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
   [Grant, D.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
   [Baum, V.; Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Schulte, L.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
   [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
   [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
   [Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Univ Berlin, Inst Phys, D-12489 Berlin, Germany.
   [Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy.
   [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
   [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
   [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
   [Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
EM lutz.koepke@uni-mainz.de
RI Tamburro, Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren,
   Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014;
   Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015;
   Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty,
   James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Kowalski,
   Marek/G-5546-2012; Taavola, Henric/B-4497-2011; 
OI Auffenberg, Jan/0000-0002-1185-9094; Koskinen,
   David/0000-0002-0514-5917; Aguilar Sanchez, Juan
   Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
   Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
   Ter-Antonyan, Samvel/0000-0002-5788-1369; Wiebusch,
   Christopher/0000-0002-6418-3008; Schukraft, Anne/0000-0002-9112-5479;
   Perez de los Heros, Carlos/0000-0002-2084-5866; Taavola,
   Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X; Carson,
   Michael/0000-0003-0400-7819; Benabderrahmane, Mohamed
   Lotfi/0000-0003-4410-5886
FU US National Science Foundation-Office of Polar Programs; US National
   Science Foundation-Physics Division; University of Wisconsin Alumni
   Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
   infrastructure at the University of Wisconsin - Madison; Open Science
   Grid (OSG) grid infrastructure; US Department of Energy; National Energy
   Research Scientific Computing Center; Louisiana Optical Network
   Initiative (LONI); National Science and Engineering Research Council of
   Canada; Swedish Research Council, Swedish Polar Research Secretariat;
   Swedish National Infrastructure for Computing (SNIC); Knut and Alice
   Wallenberg Foundation, Sweden; German Ministry for Education and
   Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research
   Department of Plasmas; Complex Interactions (Bochum), Germany
FX We acknowledge the support from the following agencies: US National
   Science Foundation-Office of Polar Programs, US National Science
   Foundation-Physics Division, University of Wisconsin Alumni Research
   Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
   at the University of Wisconsin - Madison, the Open Science Grid (OSG)
   grid infrastructure; US Department of Energy, and National Energy
   Research Scientific Computing Center, the Louisiana Optical Network
   Initiative (LONI) grid computing resources; National Science and
   Engineering Research Council of Canada; Swedish Research Council,
   Swedish Polar Research Secretariat, Swedish National Infrastructure for
   Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden;
   German Ministry for Education and Research (BMBF), Deutsche
   Forschungsgemeinschaft (DFG), Research Department of Plasmas with
   Complex Interactions (Bochum), Germany, Research Center Elementary
   Forces and Mathematical Foundations (Mainz), Germany; Fund for
   Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders
   Institute to encourage scientific and technological research in industry
   (IWT), Belgian Federal Science Policy Office (Belspo); University of
   Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for
   Promotion of Science (JSPS); the Swiss National Science Foundation
   (SNSF), Switzerland; A. Gross acknowledges support by the EU Marie Curie
   OIF Program; J. P. Rodrigues acknowledges support by the Capes
   Foundation, Ministry of Education of Brazil. We would like to thank G.
   Fogli, H. T. Janka, P, Mertsch, B. Muller, G. G. Raffelt, K. Sumiyoshi,
   I. Tamborra, and R. Tomas for providing supernova model data and for
   helpful discussions.
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   FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD NOV
PY 2011
VL 535
AR A109
DI 10.1051/0004-6361/201117810
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 858YY
UT WOS:000297841200121
ER

PT J
AU Absil, O
   Le Bouquin, JB
   Berger, JP
   Lagrange, AM
   Chauvin, G
   Lazareff, B
   Zins, G
   Haguenauer, P
   Jocou, L
   Kern, P
   Millan-Gabet, R
   Rochat, S
   Traub, W
AF Absil, O.
   Le Bouquin, J. -B.
   Berger, J. -P.
   Lagrange, A. -M.
   Chauvin, G.
   Lazareff, B.
   Zins, G.
   Haguenauer, P.
   Jocou, L.
   Kern, P.
   Millan-Gabet, R.
   Rochat, S.
   Traub, W.
TI Searching for faint companions with VLTI/PIONIER
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: interferometric; binaries: close; stars: low mass; brown
   dwarfs; planetary systems
ID INFRARED INTERFEROMETRIC SURVEY; DEBRIS DISK STARS; BETA-PICTORIS;
   STELLAR INTERFEROMETRY; CALIBRATOR STARS; ALPHA-LEONIS; CHARA ARRAY; HOT
   DUST; HR 8799; CHARA/FLUOR
AB Context. A new four-telescope interferometric instrument called PIONIER has recently been installed at VLTI. It provides improved imaging capabilities together with high precision.
   Aims. We search for low-mass companions around a few bright stars using different strategies, and determine the dynamic range currently reachable with PIONIER.
   Methods. Our method is based on the closure phase, which is the most robust interferometric quantity when searching for faint companions. We computed the chi(2) goodness of fit for a series of binary star models at different positions and with various flux ratios. The resulting chi(2) cube was used to identify the best-fit binary model and evaluate its significance, or to determine upper limits on the companion flux in case of non-detections.
   Results. No companion is found around Fomalhaut, tau Cet and Regulus. The median upper limits at 3 sigma on the companion flux ratio are respectively of 2.3 x 10(-3) (in 4 h), 3.5 x 10(-3) (in 3 h) and 5.4 x 10(-3) (in 1.5 h) on the search region extending from 5 to 100 mas. Our observations confirm that the previously detected near-infrared excess emissions around Fomalhaut and tau Cet are not related to a low-mass companion, and instead come from an extended source such as an exozodiacal disk. In the case of del Aqr, in 30 min of observation, we obtain the first direct detection of a previously known companion, at an angular distance of about 40 mas and with a flux ratio of 2.05 x 10(-2) +/- 0.16 x 10(-2). Due to the limited u, v plane coverage, its position can, however, not be unambiguously determined.
   Conclusions. After only a few months of operation, PIONIER has already achieved one of the best dynamic ranges world-wide for multi-aperture interferometers. A dynamic range up to about 1:500 is demonstrated on unresolved targets, but significant improvements are still required to reach the ultimate goal of directly detecting hot giant extrasolar planets.
C1 [Absil, O.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium.
   [Le Bouquin, J. -B.; Lagrange, A. -M.; Chauvin, G.; Lazareff, B.; Zins, G.; Jocou, L.; Kern, P.; Rochat, S.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, Grenoble, France.
   [Berger, J. -P.; Haguenauer, P.] European So Observ, Santiago 19, Chile.
   [Chauvin, G.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Millan-Gabet, R.] CALTECH, NASA Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA.
   [Traub, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Absil, O (reprint author), FRS FNRS, Brussels, Belgium.
EM absil@astro.ulg.ac.be
FU Universite Joseph Fourier (UJF, Grenoble-1); Institut de Planetologie et
   d'Astrophysique de Grenoble (IPAG, ex-LAOG); Institut National des
   Science de l'Univers (INSU); French National Research Agency (ANR)
   [ANR10-BLANC0504-01]
FX PIONIER is funded by Universite Joseph Fourier (UJF, Grenoble-1) with
   the programme TUNES-SMING, the Institut de Planetologie et
   d'Astrophysique de Grenoble (IPAG, ex-LAOG), and the Institut National
   des Science de l'Univers (INSU) with the programmes "Programme National
   de Physique Stellaire" and "Programme National de Planetologie". PIONIER
   was developed by the CRISTAL instrumental team of IPAG in collaboration
   with R. Millan-Gabet (NExScI) and W. Traub (JPL). The authors want to
   warmly thank the VLTI team. We acknowledge support from the French
   National Research Agency (ANR) through project grant ANR10-BLANC0504-01.
   This work made use of the Smithsonian/NASA Astrophysics Data System
   (ADS) and of the Centre de Donnees astronomiques de Strasbourg (CDS).
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   FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
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PY 2011
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SC Astronomy & Astrophysics
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ER

PT J
AU Bera, PP
   Head-Gordon, M
   Lee, TJ
AF Bera, Partha P.
   Head-Gordon, Martin
   Lee, Timothy J.
TI Initiating molecular growth in the interstellar medium via dimeric
   complexes of observed ions and molecules
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrochemistry; acceleration of particles; molecular processes
ID POLYCYCLIC-AROMATIC-HYDROCARBON; MATRIX-ISOLATION SPECTROSCOPY;
   DENSITY-FUNCTIONAL THEORY; FOCK PERTURBATION-THEORY; RADIATIVE
   ASSOCIATION; EXCITED-STATES; SPIN ORBITALS; AB-INITIO; CHEMISTRY;
   EMISSION
AB A feasible initiation step for particle growth in the interstellar medium (ISM) is simulated by means of ab initio quantum chemistry methods. The systems studied are dimer ions formed by pairing nitrogen containing small molecules known to exist in the ISM with ions of unsaturated hydrocarbons or vice versa. Complexation energies, structures of ensuing complexes and electronic excitation spectra of the encounter complexes are estimated using various quantum chemistry methods. Moller-Plesset perturbation theory (MP2), Z-averaged perturbation theory (ZAPT2), coupled cluster singles and doubles with perturbative triples corrections (CCSD(T)), and density functional theory (DFT) methods (B3LYP) were employed along with the correlation consistent cc-pVTZ and aug-cc-pVTZ basis sets. Two types of complexes are predicted. One type of complex has electrostatic binding with moderate (7-20 kcal mol(-1)) binding energies, that are nonetheless significantly stronger than typical van der Waals interactions between molecules of this size. The other type of complex develops strong covalent bonds between the fragments. Cyclic isomers of the nitrogen containing complexes are produced very easily by ion-molecule reactions. Some of these complexes show intense ultraviolet-visible spectra for electronic transitions with large oscillator strengths at the B3LYP, omega B97, and equations of motion coupled cluster (EOM-CCSD) levels. The open shell nitrogen containing carbonaceous complexes especially exhibit a large oscillator strength electronic transition in the visible region of the electromagnetic spectrum.
C1 [Bera, Partha P.; Lee, Timothy J.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Mountain View, CA 94035 USA.
   [Head-Gordon, Martin] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
   [Head-Gordon, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA.
RP Lee, TJ (reprint author), NASA, Space Sci & Astrobiol Div, Ames Res Ctr, MS 245-1, Mountain View, CA 94035 USA.
EM partha.p.bera@nasa.gov; Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; Bera, Partha /K-8677-2012
FU National Aeronautics and Space Administration (NASA) [08-APRA08-0050]
FX P.P.B. acknowledges a fellowship award from the National Aeronautics and
   Space Administration (NASA) postdoctoral program administered by ORAU
   for NASA. T.J.L. gratefully acknowledge support from the NASA grant
   08-APRA08-0050. The authors would like to thank the anonymous referee
   for constructive suggestions.
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   FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD NOV
PY 2011
VL 535
AR A74
DI 10.1051/0004-6361/201117103
PG 12
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SC Astronomy & Astrophysics
GA 858YY
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ER

PT J
AU Filgas, R
   Greiner, J
   Schady, P
   Kruhler, T
   Updike, AC
   Klose, S
   Nardini, M
   Kann, DA
   Rossi, A
   Sudilovsky, V
   Afonso, PMJ
   Clemens, C
   Elliott, J
   Guelbenzu, AN
   Olivares, F
   Rau, A
AF Filgas, R.
   Greiner, J.
   Schady, P.
   Kruehler, T.
   Updike, A. C.
   Klose, S.
   Nardini, M.
   Kann, D. A.
   Rossi, A.
   Sudilovsky, V.
   Afonso, P. M. J.
   Clemens, C.
   Elliott, J.
   Guelbenzu, A. Nicuesa
   Olivares E, F.
   Rau, A.
TI GRB 091127: The cooling break race on magnetic fuel
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: jets and outflows; X-rays: bursts; X-rays: individuals: GRB 091127
ID GAMMA-RAY BURST; AFTERGLOW LIGHT CURVES; OPTICAL-AFTERGLOW; HOST-GALAXY;
   THEORETICAL IMPLICATIONS; FIREBALL MODEL; JET BREAKS; SWIFT-ERA;
   PRE-SWIFT; OFF-AXIS
AB Aims. Using high-quality, broad-band afterglow data for GRB 091127, we investigate the validity of the synchrotron fireball model for gamma-ray bursts (GRBs), and infer physical parameters of the ultra-relativistic outflow.
   Methods. We used multi-wavelength (NIR to X-ray) follow-up observations obtained with GROND simultaneously in the g'r'i'z' JH filters and the XRT onboard the Swift satellite in the 0.3 to 10 keV energy range. The resulting afterglow light curve is of excellent accuracy with relative photometric errors as low as 1%, and the spectral energy distribution (SED) is well-sampled over 5 decades in energy. These data present one of the most comprehensive observing campaigns for a single GRB afterglow and allow us to test several proposed emission models and outflow characteristics in unprecedented detail.
   Results. Both the multi-color light curve and the broad-band SED of the afterglow of GRB 091127 show evidence of a cooling break moving from high to lower energies. The early light curve is well described by a broken power-law, where the initial decay in the optical/NIR wavelength range is considerably flatter than at X-rays. Detailed fitting of the time-resolved SED shows that the break is very smooth with a sharpness index of 2.2 +/- 0.2, and evolves towards lower frequencies as a power-law with index -1.23 +/- 0.06. These are the first accurate and contemporaneous measurements of both the sharpness of the spectral break and its time evolution.
   Conclusions. The measured evolution of the cooling break (gamma(c) proportional to t(similar to-1.2)) is not consistent with the predictions of the standard model, wherein gamma(c) proportional to t(similar to-0.5) is expected. A possible explanation for the observed behavior is a time dependence of the microphysical parameters, in particular the fraction of the total energy in the magnetic field epsilon(B). This conclusion provides further evidence that the standard fireball model is too simplistic, and time-dependent micro-physical parameters may be required to model the growing number of well-sampled afterglow light curves.
C1 [Filgas, R.; Greiner, J.; Schady, P.; Kruehler, T.; Nardini, M.; Sudilovsky, V.; Afonso, P. M. J.; Clemens, C.; Elliott, J.; Olivares E, F.; Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany.
   [Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
   [Updike, A. C.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
   [Updike, A. C.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
   [Updike, A. C.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
   [Updike, A. C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Klose, S.; Kann, D. A.; Rossi, A.; Guelbenzu, A. Nicuesa] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
RP Filgas, R (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
EM filgas@mpe.mpg.de
RI Rossi, Andrea/N-4674-2015; 
OI Rossi, Andrea/0000-0002-8860-6538; Kruehler, Thomas/0000-0002-8682-2384
FU DFG [HA 1850/28-1, Kl 766/16-1, SA 2001/2-1, SA 2001/1-1]; European
   Commission; Danish National Research Foundation; Deutscher Akademischer
   Austausch-Dienst (DAAD); BLANCEFLOR Boncompagni-Ludovisi, nee Bildt
   foundation; MPE
FX We thank the anonymous referee for constructive comments that helped to
   improve the paper. Part of the funding for GROND (both hardware as well
   as personnel) was generously granted from the Leibniz-Prize to Prof. G.
   Hasinger (DFG grant HA 1850/28-1). This work made use of data supplied
   by the UK Swift Science Data Centre at the University of Leicester. T.K.
   acknowledges support by the DFG cluster of excellence Origin and
   Structure of the Universe. T.K. acknowledges support by the European
   Commission under the Marie Curie Intra-European Fellowship Programme.
   The Dark Cosmology Centre is funded by the Danish National Research
   Foundation. F.O.E. acknowledges funding of his Ph.D. through the
   Deutscher Akademischer Austausch-Dienst (DAAD). S.K., D.A.K. and A.N.G.
   acknowledge support by DFG grant Kl 766/16-1. A.R. acknowledges support
   from the BLANCEFLOR Boncompagni-Ludovisi, nee Bildt foundation. M.N.
   acknowledges support by DFG grant SA 2001/2-1. P.S. acknowledges support
   by DFG grant SA 2001/1-1. A.C.U., A.N.G., D.A.K. and A.R. are grateful
   for travel funding support through MPE.
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JI Astron. Astrophys.
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SC Astronomy & Astrophysics
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UT WOS:000297841200069
ER

PT J
AU Furst, F
   Suchy, S
   Kreykenbohm, I
   Barragan, L
   Wilms, J
   Pottschmidt, K
   Caballero, I
   Kretschmar, P
   Ferrigno, C
   Rothschild, RE
AF Fuerst, F.
   Suchy, S.
   Kreykenbohm, I.
   Barragan, L.
   Wilms, J.
   Pottschmidt, K.
   Caballero, I.
   Kretschmar, P.
   Ferrigno, C.
   Rothschild, R. E.
TI Study of the many fluorescent lines and the absorption variability in GX
   301-2 with XMM-Newton
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: neutron; accretion, accretion disks; X-rays: binaries; X-rays:
   individuals: GX 301-2
ID X-RAY-EMISSION; SUPERNOVA REMNANT W49B; AUGER DECAY DATA; K-LINES; TENMA
   OBSERVATIONS; COMPTON SHOULDER; NEUTRON-STAR; LIGHT-CURVE; VELA X-1;
   IRON
AB We present an in-depth study of the high mass X-ray binary (HMXB) GX 301-2 during its pre-periastron flare using data from the XMM-Newton satellite. The energy spectrum shows a power law continuum absorbed by a large equivalent hydrogen column on the order of 10(24) cm(-2) and a prominent Fe K alpha fluorescent emission line. Besides the Fe K alpha line, evidence for Fe K beta, Ni K alpha, Ni K beta, S K alpha, Ar K alpha, Ca K alpha, and Cr K alpha fluorescent lines is found. The observed line strengths are consistent with fluorescence in a cold absorber. This is the first time that Cr K alpha is seen in emission in the X-ray spectrum of a HMXB. In addition to the modulation by the strong pulse period of similar to 685 s the source is highly variable and shows different states of activity. We perform time-resolved as well as pulse-to-pulse resolved spectroscopy to investigate differences between these states of activity. We find that fluorescent line fluxes are strongly variable and generally follow the overall flux. The N-H value is variable by a factor of 2, but not correlated to continuum normalization. We find an interval of low flux in the light curve in which the pulsations cease almost completely, without any indication of an increasing absorption column. We investigate this dip in detail and argue that it is most likely that during the dip the accretion ceased and the afterglow of the fluorescent iron accounted for the main portion of the X-ray flux. A similar dip was found earlier in RXTE data, and we compare our findings to these results.
C1 [Fuerst, F.; Kreykenbohm, I.; Barragan, L.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
   [Fuerst, F.; Kreykenbohm, I.; Barragan, L.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
   [Suchy, S.; Rothschild, R. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
   [Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
   [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
   [Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
   [Caballero, I.] Univ Paris Diderot, CEA, CNRS, CEA Saclay,DSM,IRFU,SAp,UMR AIM 7158, F-91191 Gif Sur Yvette, France.
   [Kretschmar, P.] European Space Astron Ctr, ISOC, Villanueva De La Canada 28691, Spain.
   [Ferrigno, C.] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
RP Furst, F (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, Sternwartstr 7, D-96049 Bamberg, Germany.
EM felix.fuerst@sternwarte.uni-erlangen.de
RI Ferrigno, Carlo/H-4139-2012; Wilms, Joern/C-8116-2013; Kreykenbohm,
   Ingo/H-9659-2013; 
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803;
   Kretschmar, Peter/0000-0001-9840-2048
FU Bundesministerium fur Wirtschaft und Technologie through DLR [50
   OR0808]; Bundesministerium fur Wirtschaft und Technologie via DAAD;
   European Commission [ITN215212]; NASA [NAS5-30720, NNX08AX83G]; French
   Space Agency CNES through CNRS; ESA; NASA
FX We thank the anonymous referee for her/his useful comments. This work
   was supported by the Bundesministerium fur Wirtschaft und Technologie
   through DLR grant 50 OR0808, via a DAAD fellowship, and has been
   partially funded by the European Commission under the 7th Framework
   Program under contract ITN215212 "Black Hole Universe". S. S.
   acknowledges support by NASA contract NAS5-30720 and NNX08AX83G. I. C.
   acknowledges financial support from the French Space Agency CNES through
   CNRS. F. F. thanks the colleagues at UCSD and GSFC for their
   hospitality. We have made use of NASA's Astrophysics Data System. This
   work is based on observations obtained with XMM-Newton, an ESA science
   mission with instruments and contributions directly funded by ESA Member
   States and NASA. We made use of results provided by the ASM/RXTE teams
   at MIT and at the RXTE SOF and GOF at NASA's GSFC. We used the ISIS
   software package provided by MIT for this work. We especially like to
   thank J. C. Houck and J. E. Davis for their restless work to improve
   ISIS and S-Lang.
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JI Astron. Astrophys.
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ER

PT J
AU Le Bouquin, JB
   Berger, JP
   Lazareff, B
   Zins, G
   Haguenauer, P
   Jocou, L
   Kern, P
   Millan-Gabet, R
   Traub, W
   Absil, O
   Augereau, JC
   Benisty, M
   Blind, N
   Bonfils, X
   Bourget, P
   Delboulbe, A
   Feautrier, P
   Germain, M
   Gitton, P
   Gillier, D
   Kiekebusch, M
   Kluska, J
   Knudstrup, J
   Labeye, P
   Lizon, JL
   Monin, JL
   Magnard, Y
   Malbet, F
   Maurel, D
   Menard, F
   Micallef, M
   Michaud, L
   Montagnier, G
   Morel, S
   Moulin, T
   Perraut, K
   Popovic, D
   Rabou, P
   Rochat, S
   Rojas, C
   Roussel, F
   Roux, A
   Stadler, E
   Stefl, S
   Tatulli, E
   Ventura, N
AF Le Bouquin, J. -B.
   Berger, J. -P.
   Lazareff, B.
   Zins, G.
   Haguenauer, P.
   Jocou, L.
   Kern, P.
   Millan-Gabet, R.
   Traub, W.
   Absil, O.
   Augereau, J. -C.
   Benisty, M.
   Blind, N.
   Bonfils, X.
   Bourget, P.
   Delboulbe, A.
   Feautrier, P.
   Germain, M.
   Gitton, P.
   Gillier, D.
   Kiekebusch, M.
   Kluska, J.
   Knudstrup, J.
   Labeye, P.
   Lizon, J. -L.
   Monin, J. -L.
   Magnard, Y.
   Malbet, F.
   Maurel, D.
   Menard, F.
   Micallef, M.
   Michaud, L.
   Montagnier, G.
   Morel, S.
   Moulin, T.
   Perraut, K.
   Popovic, D.
   Rabou, P.
   Rochat, S.
   Rojas, C.
   Roussel, F.
   Roux, A.
   Stadler, E.
   Stefl, S.
   Tatulli, E.
   Ventura, N.
TI PIONIER: a 4-telescope visitor instrument at VLTI
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: interferometers; techniques: interferometric;
   techniques: high angular resolution; instrumentation: high angular
   resolution
ID INFRARED INTERFEROMETRIC SURVEY; OPTICS BEAM COMBINER;
   INTEGRATED-OPTICS; ASTRONOMICAL INTERFEROMETRY; STELLAR INTERFEROMETRY;
   CALIBRATOR STARS; HOT DUST; T-TAURI; DISKS; CHARA/FLUOR
AB Context. PIONIER stands for Precision Integrated-Optics Near-infrared Imaging ExpeRiment. It combines four 1.8m Auxilliary Telescopes or four 8m Unit Telescopes of the Very Large Telescope Interferometer (ESO, Chile) using an integrated optics combiner. The instrument was integrated at IPAG in December 2009 and commissioned at the Paranal Observatory in October 2010. It has provided scientific observations since November 2010.
   Aims. In this paper, we explain the instrumental concept and describe the standard operational modes and the data reduction strategy. We present the typical performance and discuss how to improve them.
   Methods. This paper is based on laboratory data obtained during the integrations at IPAG, as well as on-sky data gathered during the commissioning at VLTI. We illustrate the imaging capability of PIONIER on the binaries delta Sco and HIP11231.
   Results. PIONIER provides six visibilities and three independent closure phases in the H band, either in a broadband mode or with a low spectral dispersion (R = 40), using natural light (i.e. unpolarized). The limiting magnitude is Hmag = 7 in dispersed mode under median atmospheric conditions (seeing <1 '', tau(0) > 3ms) with the 1.8m Auxiliary Telescopes. We demonstrate a precision of 0.5 deg on the closure phases. The precision on the calibrated visibilities ranges from 3% to 15% depending on the atmospheric conditions.
   Conclusions. PIONIER was installed and successfully tested as a visitor instrument for the VLTI. It permits high angular resolution imaging studies at an unprecedented level of sensitivity. The successful combination of the four 8m Unit Telescopes in March 2011 demonstrates that VLTI is ready for four-telescope operation.
C1 [Le Bouquin, J. -B.; Lazareff, B.; Zins, G.; Jocou, L.; Kern, P.; Augereau, J. -C.; Blind, N.; Bonfils, X.; Delboulbe, A.; Feautrier, P.; Germain, M.; Gillier, D.; Kluska, J.; Monin, J. -L.; Magnard, Y.; Malbet, F.; Maurel, D.; Menard, F.; Micallef, M.; Michaud, L.; Moulin, T.; Perraut, K.; Rabou, P.; Rochat, S.; Roussel, F.; Roux, A.; Stadler, E.; Tatulli, E.; Ventura, N.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, Grenoble, France.
   [Berger, J. -P.; Haguenauer, P.; Bourget, P.; Gitton, P.; Montagnier, G.; Morel, S.; Rojas, C.; Stefl, S.] European Org Astron Res So Hemisphere ESO, Santiago 19, Chile.
   [Millan-Gabet, R.] CALTECH, NASA Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA.
   [Traub, W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Benisty, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Absil, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
   [Kiekebusch, M.; Knudstrup, J.; Lizon, J. -L.; Popovic, D.] European Org Astron Res So Hemisphere ESO, D-85748 Garching, Germany.
   [Labeye, P.] CEA, LETI, F-38054 Grenoble 9, France.
RP Le Bouquin, JB (reprint author), UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, Grenoble, France.
EM jean-baptiste.lebouquin@obs.ujf-grenoble.fr
OI Bonfils, Xavier/0000-0001-9003-8894
FU Universite Joseph Fourier (UJF, Grenoble); Institut de Planetologie et
   d'Astrophysique de Grenoble; Agence Nationale pour la Recherche;
   Institut National des Science de l'Univers (INSU); Programme National de
   Planetologie
FX PIONIER is funded by the Universite Joseph Fourier (UJF, Grenoble)
   through its Poles TUNES and SMING and the vice-president of research,
   the Institut de Planetologie et d'Astrophysique de Grenoble, the "Agence
   Nationale pour la Recherche" with the program ANR EXOZODI, and the
   Institut National des Science de l'Univers (INSU) with the programs
   "Programme National de Physique Stellaire" and "Programme National de
   Planetologie". The integrated optics beam combiner is the result of a
   collaboration between IPAG and CEA-LETI based on CNES R&T funding. The
   authors want to warmly thank all the people involved in the VLTI
   project. This work is based on observations made with the ESO
   telescopes. It made use of the Smithsonian/NASA Astrophysics Data System
   (ADS) and of the Centre de Donnees astronomiques de Strasbourg (CDS).
   All calculations and graphics were performed with the freeware Yorick.
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PY 2011
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PT J
AU Rambaux, N
   Castillo-Rogez, J
   Dehant, V
   Kuchynka, P
AF Rambaux, N.
   Castillo-Rogez, J.
   Dehant, V.
   Kuchynka, P.
TI Constraining Ceres' interior from its rotational motion
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: dynamical evolution and stability; celestial
   mechanics
ID ICY SATELLITES; TIDAL DISSIPATION; NUTATION SERIES; MOLTEN CORE; EARTH;
   EUROPA; EVOLUTION; DIFFERENTIATION; DIMENSIONS; JUPITERS
AB Context. Ceres is the most massive body of the asteroid belt and contains about 25 wt.% (weight percent) of water. Understanding its thermal evolution and assessing its current state are major goals of the Dawn mission. Constraints on its internal structure can be inferred from various types of observations. In particular, detailed knowledge of the rotational motion can help constrain the mass distribution inside the body, which in turn can lead to information about its geophysical history.
   Aims. We investigate the signature of internal processes on Ceres rotational motion and discuss future measurements that can possibly be performed by the spacecraft Dawn and will help to constrain Ceres' internal structure.
   Methods. We compute the polar motion, precession-nutation, and length-of-day variations. We estimate the amplitudes of the rigid and non-rigid responses for these various motions for models of Ceres' interior constrained by shape data and surface properties.
   Results. As a general result, the amplitudes of oscillations in the rotation appear to be small, and their determination from spaceborne techniques will be challenging. For example, the amplitudes of the semi-annual and annual nutations are around similar to 364 and similar to 140 milli-arcseconds, and they show little variation within the parametric space of interior models envisioned for Ceres.
   Conclusions. Owing to the small amplitudes of the nutation and the very long-period of the precession motion, the measurements of the rotational variations will be challenging to obtain. We also estimate the timescale for Ceres' orientation to relax to a generalized Cassini state, and find that the tidal dissipation within that object has probably been too small to drive any significant damping of its obliquity since formation. However, combining the shape and gravity observations of Dawn offers the prospect to identify departures of non-hydrostaticity on both global and regional scales, which will be instrumental in constraining Ceres' past and current thermal state. We also discuss the existence of a possible Chandler mode in the rotational motion of Ceres, whose potential excitation by endogenic and/or exogenic processes may help us to detect the presence of liquid reservoirs within the asteroid.
C1 [Rambaux, N.] Univ Paris 06, F-75252 Paris 05, France.
   [Rambaux, N.; Kuchynka, P.] CNRS, Observ Paris, IMCCE, UMR 8028, F-75014 Paris, France.
   [Castillo-Rogez, J.; Kuchynka, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Dehant, V.] Royal Observ Belgium, B-1180 Brussels, Belgium.
RP Rambaux, N (reprint author), Univ Paris 06, F-75252 Paris 05, France.
EM nicolas.rambaux@imcce.fr; julie.c.castillo@jpl.nasa.gov;
   kuchynka@imcce.fr
FU Jet Propulsion Laboratory, California Institute of Technology; Paris
   Observatory
FX The authors wish to thank Jim Williams (JPL) and Richard Gross (JPL) for
   valuable discussions on the secular orbits of asteroids and the
   excitation of the Chandler wobble. The authors are also thankful to the
   anonymous reviewers, who helped improve the quality of this manuscript.
   Part of this work was conducted at the Jet Propulsion Laboratory,
   California Institute of Technology, under contract to NASA. Government
   sponsorship acknowledged. All rights reserved. This research benefits
   from the financial support of the Paris Observatory (2010).
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SN 0004-6361
EI 1432-0746
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JI Astron. Astrophys.
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PY 2011
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PT J
AU Woodard, SE
   Taylor, BD
   Jones, TW
   Shams, QA
   Lyons, F
   Henderson, DJ
AF Woodard, Stanley E.
   Taylor, Bryant D.
   Jones, Thomas W.
   Shams, Qamar A.
   Lyons, Frankel
   Henderson, Donald J.
TI Method to Have Multilayer Thermal Insulation Provide Damage Detection
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/ASME/ASCE/AHS 29th Structures, Structural Dynamics and Materials
   Conference
CY APR 23-26, 2007
CL Honolulu, HI
SP AIAA, ASME, ASCE, AHS
AB Spacecraft multilayer thermal insulation here to date has been used to reduce thermal radiation heat losses. Each layer is a thin layer of material, such as Mylar, coated with a reflective and electrically conductive material like aluminum. A method to create a wireless damage-detection array using the insulation has been developed. One layer of the insulation is designed as an array of passive open-circuit electrically conductive and reflective spiral patterns that are capable of storing electrical and magnetic energy when powered via an external oscillating magnetic field supplied by an antenna. Once electrically active, each pattern produces a harmonic magnetic field. No electrical connections are used between the patterns, on the patterns or to the patterns thereby allowing each pattern to be independent and also eliminating one cause of failure to circuits. The responding field frequency changes if any pattern is damaged. The spiral-pattern design provides sufficient area coverage for thermal insulation. Other insulation layers are designed to allow the responding magnetic fields to permeate the insulation layers. Arrays have been tested using hypervelocity impact projectiles of 1-3.6 mm diameter with speeds ranging from 6.7-7.1 km/s.
C1 [Woodard, Stanley E.; Jones, Thomas W.; Shams, Qamar A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Taylor, Bryant D.] Swales Aerosp, Hampton, VA 23681 USA.
   [Lyons, Frankel] ESCG Hamilton Sundstrand, Houston, TX 77058 USA.
   [Henderson, Donald J.] NASA, White Sands Test Facil, Las Cruces, NM 88012 USA.
EM b.d.taylor@larc.nasa.gov; t.w.jones@larc.nasa.gov;
   q.a.shams@larc.nasa.gov; frankel.lyons-1@nasa.gov;
   donald.j.henderson@nasa.gov
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PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD NOV-DEC
PY 2011
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BP 920
EP 930
DI 10.2514/1.44400
PG 11
WC Engineering, Aerospace
SC Engineering
GA 862UZ
UT WOS:000298120900003
ER

PT J
AU Osipov, VV
   Daigle, MJ
   Muratov, CB
   Foygel, M
   Smelyanskiy, VN
   Watson, MD
AF Osipov, Viatcheslav V.
   Daigle, Matthew J.
   Muratov, Cyrill B.
   Foygel, Michael
   Smelyanskiy, Vadim N.
   Watson, Michael D.
TI Dynamical Model of Rocket Propellant Loading with Liquid Hydrogen
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB A dynamical model describing the multistage process of rocket propellant loading has been developed. It accounts for both the nominal and faulty regimes of cryogenic fuel loading when liquid hydrogen is moved from a storage tank to an external tank via a transfer line. By employing basic conservation laws, the reduced lumped-parameter model takes into consideration the major multiphase mass and energy exchange processes involved, such as highly nonequilibrium condensation evaporation of hydrogen, pressurization of the tanks, and liquid hydrogen and hydrogen vapor flows in the presence of pressurizing helium gas. A self-consistent theory of dynamical condensation evaporation has been developed that incorporates heat flow by both conduction and convection through the liquid/vapor interface inside the tanks. A simulation has been developed in MATLAB for a generic refueling system that involves the solution of a system of ordinary integro-differential equations. The results of these simulations are in good agreement with space shuttle refueling data.
C1 [Osipov, Viatcheslav V.] MCT Inc, Moffett Field, CA 94035 USA.
   [Daigle, Matthew J.] Univ Calif Santa Cruz, Intelligent Syst Div, Moffett Field, CA 94035 USA.
   [Muratov, Cyrill B.] New Jersey Inst Technol, Newark, NJ 07102 USA.
   [Foygel, Michael] SGT Inc, Newark, NJ 07102 USA.
   [Smelyanskiy, Vadim N.] NASA, Ames Res Ctr, Appl Phys Grp, Moffett Field, CA 94035 USA.
   [Watson, Michael D.] NASA, George C Marshall Space Flight Ctr, ISHM, Huntsville, AL 35805 USA.
   [Watson, Michael D.] NASA, George C Marshall Space Flight Ctr, Sensors Branch, Huntsville, AL 35805 USA.
RP Osipov, VV (reprint author), NASA, Ames Res Ctr, Appl Phys Grp, Moffett Field, CA 94035 USA.
OI Daigle, Matthew/0000-0002-4616-3302
NR 14
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U2 6
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD NOV-DEC
PY 2011
VL 48
IS 6
BP 987
EP 998
DI 10.2514/1.52587
PG 12
WC Engineering, Aerospace
SC Engineering
GA 862UZ
UT WOS:000298120900008
ER

PT J
AU Lafleur, JM
   Cerimele, CJ
AF Lafleur, Jarret M.
   Cerimele, Christopher J.
TI Mars Entry Bank Profile Design for Terminal State Optimization
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA Atmospheric Flight Mechanics Conference and Exhibit
CY AUG 18-21, 2008
CL Honolulu, HI
SP AIAA
AB One critical technical challenge facing future Mars missions is that of entry, descent, and landing for high-ballistic-coefficient heavy-robotic or human-class payloads. To benchmark best possible entry scenarios for the evaluation of potential system designs, a parametric study is conducted to optimize the terminal state of Mars entry trajectories. The terminal state is envisioned as one appropriate for initiation of terminal descent via parachute or other means. A particle swarm optimizer varies entry flight-path angle and ten bank profile points to find maximum-terminal-altitude trajectories for 960 combinations of vehicle ballistic coefficient, lift-to-drag ratio, entry velocity, terminal Mach number, and minimum allowable altitude. Characteristics of optimized trajectories are observed, and optimum terminal altitudes are compiled into parametric, vehicle-independent contour plots. Vehicle-specific contours are then overlaid on the plots, permitting estimation of maximum terminal altitude and identification of feasible masses for various vehicle shapes. For example, data show that an Apollo-class capsule entering the Martian atmosphere at 4.7 km/s can reach a maximum altitude of 18.3 km at Mach 5. Along with providing useful data for the design of future vehicles, this study indicates that kilometers of gain in terminal altitude are possible when bank-angle modulation is employed over a full lift-up profile.
C1 [Lafleur, Jarret M.; Cerimele, Christopher J.] NASA, Lyndon B Johnson Space Ctr, Flight Mech & Trajectory Design Branch EG5, Houston, TX 77058 USA.
RP Lafleur, JM (reprint author), NASA, Lyndon B Johnson Space Ctr, Flight Mech & Trajectory Design Branch EG5, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM jarret.m.lafleur@gatech.edu
NR 25
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U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD NOV-DEC
PY 2011
VL 48
IS 6
BP 1012
EP 1024
DI 10.2514/1.51944
PG 13
WC Engineering, Aerospace
SC Engineering
GA 862UZ
UT WOS:000298120900010
ER

PT J
AU Montenbruck, O
   Rozkov, S
   Semenov, A
   Gomez, SF
   Nasca, R
   Cacciapuoti, L
AF Montenbruck, Oliver
   Rozkov, Sergey
   Semenov, Alexander
   Gomez, Susan F.
   Nasca, Rosario
   Cacciapuoti, Luigi
TI Orbit Determination and Prediction of the International Space Station
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB The International Space Station is equipped with Global Positioning System receivers that provide real-time position information at the 10 m accuracy level. In preparation of the Atomic Clock Ensemble in Space experiment, measurements from Russian and American receivers have been used to assess the navigation accuracy that can be achieved through postprocessing of navigation solutions and raw data in a precise orbit determination process. In addition, the capability to accurately forecast the space station orbit for operation of microwave and laser terminals has been studied. It is shown that the orbit can be reconstructed with a I m position accuracy and a 1 minis velocity accuracy even from single-frequency Global Positioning System measurements. For the test period in mid 2006, short arc orbit predictions with a median error of 20 and 70 m could be obtained over forecast intervals of 6 and 12 h, respectively. The navigation accuracy obtained is compatible with the mission requirements for the relativistic correction of the atomic clocks and the quick look clock performance monitoring.
C1 [Montenbruck, Oliver] German Aerosp Ctr, DLR, GNSS Technol & Nav, D-82234 Wessling, Germany.
   [Rozkov, Sergey; Semenov, Alexander] RSC Energia, Moscow 141070, Russia.
   [Gomez, Susan F.] NASA, Lyndon B Johnson Space Ctr, ISS GNC, Houston, TX 77058 USA.
   [Nasca, Rosario] ESA, Payload Facil Dev & Syst Engn Off, Directorate Human Spaceflight, NL-2200 AG Noordwijk, Netherlands.
   [Cacciapuoti, Luigi] ESA, Res & Sci Support Dept, Sci Directorate, ACES Project, NL-2200 AG Noordwijk, Netherlands.
RP Montenbruck, O (reprint author), German Aerosp Ctr, DLR, GNSS Technol & Nav, D-82234 Wessling, Germany.
OI Montenbruck, Oliver/0000-0003-4783-745X
FU ESA [16242/02/NL/JS]
FX This study was supported by Astrium under ESA contract 16242/02/NL/JS.
   The authors are grateful to NASA and RSC Energia for provision of the
   ASN-M and SIGI flight data as well as the auxiliary telemetry used in
   this study. The contributions of Achim Helm (Astrium) and Martin Wermuth
   (DLR, German Aerospace Center) in the data analysis and preparation of
   the manuscript are specifically acknowledged and appreciated.
NR 24
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U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD NOV-DEC
PY 2011
VL 48
IS 6
BP 1055
EP 1067
DI 10.2514/1.52657
PG 13
WC Engineering, Aerospace
SC Engineering
GA 862UZ
UT WOS:000298120900014
ER

PT J
AU Kharuk, VI
   Dvinskaya, ML
   Im, ST
   Ranson, KJ
AF Kharuk, V. I.
   Dvinskaya, M. L.
   Im, S. T.
   Ranson, K. J.
TI The Potential Impact of CO2 and Air Temperature Increases on Krummholz
   Transformation into Arborescent Form in the Southern Siberian Mountains
SO ARCTIC ANTARCTIC AND ALPINE RESEARCH
LA English
DT Article
ID FOREST-TUNDRA ECOTONE; GLACIER-NATIONAL-PARK; TREE-LINE EVOLUTION;
   CLIMATE-CHANGE; EVERGREEN CONIFERS; SWEDISH SCANDES; GROWTH; USA;
   ELEVATION; ECOSYSTEM
AB Trees in the southern Siberian Mountains forest-tundra ecotone have considerably increased their radial and apical growth increments during the last few decades. This leads to the widespread vertical transformation of mat and prostrate krummholz forms of larch (Larix sibirica Ledeb) and Siberian pine (Pinus sibirica Du Tour). An analysis of the radial growth increments showed that these transformations began in the mid-1980s. Larch showed a greater resistance to the harsh alpine environment and attained a vertical growth form in areas where Siberian pine is still krummholz. Upper larch treeline is >= 10 m higher than Siberian pine treeline. Observed apical and radial growth increment increases were correlated with CO2 concentration (r = 0.83-0.87), summer temperatures (r = 0.55-0.64), and "cold period" (i.e. September May) air temperatures (r = 0.36-0.37). Positive correlation between growth increments and winter precipitation was attributed to snow cover protection for trees during wintertime.
C1 [Kharuk, V. I.; Dvinskaya, M. L.; Im, S. T.] VN Sukachev Inst Forest, Krasnoyarsk, Russia.
   [Ranson, K. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kharuk, VI (reprint author), VN Sukachev Inst Forest, Krasnoyarsk, Russia.
EM kharuk@ksc.krasn.ru
RI Ranson, Kenneth/G-2446-2012
OI Ranson, Kenneth/0000-0003-3806-7270
FU Siberian Branch Russian Academy of Science [23.3.33]; NASA's Science
   Mission Directorate
FX This research was supported in part by the Siberian Branch Russian
   Academy of Science Program # 23.3.33 and NASA's Science Mission
   Directorate.
NR 47
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PU INST ARCTIC ALPINE RES
PI BOULDER
PA UNIV COLORADO, BOULDER, CO 80309 USA
SN 1523-0430
EI 1938-4246
J9 ARCT ANTARCT ALP RES
JI Arct. Antarct. Alp. Res.
PD NOV
PY 2011
VL 43
IS 4
BP 593
EP 600
DI 10.1657/1938-4246-43.4.593
PG 8
WC Environmental Sciences; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 871FD
UT WOS:000298722400009
ER

PT J
AU Van Cooten, S
   Kelleher, KE
   Howard, K
   Zhang, J
   Gourley, JJ
   Kain, JS
   Nemunaitis-Monroe, K
   Flamig, Z
   Moser, H
   Arthur, A
   Langston, C
   Kolar, R
   Hong, Y
   Dresback, K
   Tromble, E
   Vergara, H
   Luettich, RA
   Blanton, B
   Lander, H
   Galluppi, K
   Losego, JP
   Blain, CA
   Thigpen, J
   Mosher, K
   Figurskey, D
   Moneypenny, M
   Blaes, J
   Orrock, J
   Bandy, R
   Goodall, C
   Kelley, JGW
   Greenlaw, J
   Wengren, M
   Eslinger, D
   Payne, J
   Olmi, G
   Feldt, J
   Schmidt, J
   Hamill, T
   Bacon, R
   Stickney, R
   Spence, L
AF Van Cooten, Suzanne
   Kelleher, Kevin E.
   Howard, Kenneth
   Zhang, Jian
   Gourley, Jonathan J.
   Kain, John S.
   Nemunaitis-Monroe, Kodi
   Flamig, Zac
   Moser, Heather
   Arthur, Ami
   Langston, Carrie
   Kolar, Randall
   Hong, Yang
   Dresback, Kendra
   Tromble, Evan
   Vergara, Humberto
   Luettich, Richard A., Jr.
   Blanton, Brian
   Lander, Howard
   Galluppi, Ken
   Losego, Jessica Proud
   Blain, Cheryl Ann
   Thigpen, Jack
   Mosher, Katie
   Figurskey, Darin
   Moneypenny, Michael
   Blaes, Jonathan
   Orrock, Jeff
   Bandy, Rich
   Goodall, Carin
   Kelley, John G. W.
   Greenlaw, Jason
   Wengren, Micah
   Eslinger, Dave
   Payne, Jeff
   Olmi, Geno
   Feldt, John
   Schmidt, John
   Hamill, Todd
   Bacon, Robert
   Stickney, Robert
   Spence, Lundie
TI THE CI-FLOW PROJECT A System for Total Water Level Prediction from the
   Summit to the Sea
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID NATIONAL-WEATHER-SERVICE; 3RD-GENERATION WAVE MODEL; COASTAL REGIONS;
   REAL-TIME; PROGRAM; RIVER; WIND; VALIDATION; PRESSURE; PLANS
AB The objective of the Coastal and Inland Flooding Observation and Warning (CI-FLOW) project is to prototype new hydrometeorologic techniques to address a critical NOAA service gap: routine total water level predictions for tidally influenced watersheds. Since February 2000, the project has focused on developing a coupled modeling system to accurately account for water at all locations in a coastal watershed by exchanging data between atmospheric, hydrologic, and hydrodynamic models. These simulations account for the quantity of water associated with waves, tides, storm surge, rivers, and rainfall, including interactions at the tidal/surge interface. Within this project, CI-FLOW addresses the following goals: i) apply advanced weather and oceanographic monitoring and prediction techniques to the coastal environment; ii) prototype an automated hydrometeorologic data collection and prediction system; iii) facilitate interdisciplinary and multiorganizational collaborations; and iv) enhance techniques and technologies that improve actionable hydrologic/hydrodynamic information to reduce the impacts of coastal flooding. Results are presented for Hurricane Isabel (2003), Hurricane Earl (2010), and Tropical Storm Nicole (2010) for the Tar-Pamlico and Neuse River basins of North Carolina. This area was chosen, in part, because of the tremendous damage inflicted by Hurricanes Dennis and Floyd (1999). The vision is to transition CI-FLOW research findings and tethnologies to other U.S. coastal watersheds. (Page 1427)
C1 [Nemunaitis-Monroe, Kodi; Flamig, Zac; Moser, Heather; Arthur, Ami; Langston, Carrie] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73019 USA.
   [Kolar, Randall; Hong, Yang; Dresback, Kendra; Tromble, Evan; Vergara, Humberto] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
   [Luettich, Richard A., Jr.] Univ N Carolina Chapel Hill, Inst Marine Sci, Morehead City, NC USA.
   [Blanton, Brian; Lander, Howard; Galluppi, Ken; Losego, Jessica Proud] Univ N Carolina, RENCI, Chapel Hill, NC USA.
   [Blain, Cheryl Ann] USN, Div Oceanog, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS USA.
   [Thigpen, Jack; Mosher, Katie] N Carolina Sea Grant, Raleigh, NC USA.
   [Figurskey, Darin; Moneypenny, Michael; Blaes, Jonathan; Orrock, Jeff] NOAA NWS Forecast Off, Raleigh, NC USA.
   [Bandy, Rich; Goodall, Carin] NOAA NWS Forecast Off, Newport, NC USA.
   [Kelley, John G. W.; Greenlaw, Jason; Wengren, Micah] NOAA NOS Coast Survey Dev Lab, Silver Spring, MD USA.
   [Eslinger, Dave; Payne, Jeff; Olmi, Geno] NOAA CSC, Charleston, SC USA.
   [Feldt, John; Schmidt, John; Hamill, Todd] NOAA NWS SE River Forecast Ctr, Peachtree City, GA USA.
   [Bacon, Robert] S Carolina Sea Grant, Charleston, SC USA.
   [Stickney, Robert] Texas Sea Grant, College Stn, TX USA.
   [Spence, Lundie] Ctr Ocean Sci Educ Excellence SE, Charleston, SC USA.
   [Van Cooten, Suzanne; Kelleher, Kevin E.; Howard, Kenneth; Zhang, Jian; Gourley, Jonathan J.; Kain, John S.; Nemunaitis-Monroe, Kodi; Flamig, Zac; Moser, Heather; Arthur, Ami; Langston, Carrie] NOAA NSSL, Norman, OK USA.
RP Van Cooten, S (reprint author), NSSL, 120 David L Boren Blvd, Norman, OK 73072 USA.
EM suzanne.van.cooten@noaa.gov
RI Hong, Yang/D-5132-2009; Kelleher, Kevin/L-6520-2015; Gourley,
   Jonathan/C-7929-2016
OI Hong, Yang/0000-0001-8720-242X; Gourley, Jonathan/0000-0001-7363-3755
FU Department of Homeland Security, Center of Excellence
   [2008-ST-061-ND0001-02]; NOAA IOOS [NA07NOS4730212]; NOAA's Office of
   Oceanic and Atmospheric Research under NOAA-University of Oklahoma
   [NA17RJ1227]; U.S. Department of Commerce; NSSL
FX The CI-FLOW project would not have been possible without the pioneering
   discussions between NSSL and NOAA Sea Grant. Thanks to the members of
   the vision team: Ron Baird, director of NOAA Sea Grant (retired), and
   James Kimpel, director of NSSL (retired). Additional thanks go to our
   advocates and funding sponsors, including Andy Shepherd of NOAA's
   National Undersea Research Program, NOAA in the Carolinas, the NOAA
   Southeast and Caribbean Regional Team, and NOAA's CSC. Support for
   ADCIRC was provided, in part, through the Department of Homeland
   Security, Center of Excellence Contract 2008-ST-061-ND0001-02, the NOAA
   IOOS Program through Contract NA07NOS4730212, the Cooperative Institute
   for Mesoscale Meteorological Studies' cooperative agreement funding by
   NOAA's Office of Oceanic and Atmospheric Research under NOAA-University
   of Oklahoma Cooperative Agreement NA17RJ1227 U.S. Department of
   Commerce, and NSSL, which the authors gratefully acknowledge. Any
   opinions, findings, conclusions, and recommendations expressed in this
   material are those of the authors and do not necessarily reflect those
   of the funding agencies. The authors also appreciate the comments and
   suggestions from three anonymous reviewers, which improved the structure
   of this manuscript.
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PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD NOV
PY 2011
VL 92
IS 11
BP 1427
EP +
DI 10.1175/2011BAMS3150.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 863ZA
UT WOS:000298205600008
ER

PT J
AU Fletcher, LE
   Conley, CA
   Valdivia-Silva, JE
   Perez-Montano, S
   Condori-Apaza, R
   Kovacs, GTA
   Glavin, DP
   McKay, CP
AF Fletcher, Lauren E.
   Conley, Catharine A.
   Valdivia-Silva, Julio E.
   Perez-Montano, Saul
   Condori-Apaza, Renee
   Kovacs, Gregory T. A.
   Glavin, Daniel P.
   McKay, Christopher P.
TI Determination of low bacterial concentrations in hyperarid Atacama
   soils: comparison of biochemical and microscopy methods with real-time
   quantitative PCR
SO CANADIAN JOURNAL OF MICROBIOLOGY
LA English
DT Article
DE soil DNA; real-time qPCR; hyperarid environment; Atacama Desert
ID POLYMERASE-CHAIN-REACTION; RIBOSOMAL-RNA GENE; MICROBIAL LIFE; MEDIATED
   AMPLIFICATION; ENVIRONMENTAL-SAMPLES; ESCHERICHIA-COLI; PLASMID DNA;
   DESERT; SEDIMENTS; ENUMERATION
AB Hyperarid Atacama soils are reported to contain significantly reduced numbers of microbes per gram of soil relative to soils from other environments. Molecular methods have been used to evaluate microbial populations in hyperarid Atacama soils; however, conflicting results across the various studies, possibly caused by this low number of microorganisms and consequent biomass, suggest that knowledge of expected DNA concentrations in these soils becomes important to interpreting data from any method regarding microbial concentrations and diversity. In this paper we compare the number of bacteria per gram of Atacama Desert soils determined by real-time quantitative polymerase chain reaction with the number of bacteria estimated by the standard methods of phospholipids fatty acid analysis, adenine composition (determined by liquid chromatography time-of-flight mass spectrometry), and SYBR-green microscopy. The number determined by real-time quantitative polymerase chain reaction as implemented in this study was several orders of magnitude lower than that determined by the other three methods and probably underestimates the concentrations of soil bacteria, most likely because of soil binding during the DNA extraction methods. However, the other methods very possibly overestimate the bacteria concentrations owing to desiccated, intact organisms, which would stain positive in microscopy and preserve both adenine and phospholipid fatty acid for the other methods.
C1 [Fletcher, Lauren E.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
   [Fletcher, Lauren E.; Valdivia-Silva, Julio E.; Perez-Montano, Saul; McKay, Christopher P.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Conley, Catharine A.] NASA Headquarters, Sci Mission Directorate, Planetary Sci Div, Washington, DC 20546 USA.
   [Perez-Montano, Saul] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA.
   [Condori-Apaza, Renee] Univ Nacl San Agustin, Arequipa, Peru.
   [Kovacs, Gregory T. A.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
   [Glavin, Daniel P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Fletcher, LE (reprint author), Univ Oxford, Clarendon Lab, Pk Rd, Oxford OX1 3PU, England.
EM Lauren@atm.ox.ac.uk
RI Glavin, Daniel/D-6194-2012; 
OI Glavin, Daniel/0000-0001-7779-7765; CONDORI APAZA,
   RENEE/0000-0002-1097-5026
FU Universidad Nacional de San Agustin located in Arequipa, Peru; NASA
   ASTEP
FX We would like to thank Dr. Benito Gomez for many years of support and
   access to the Yungay Desert Research Station, Chile; Dr. Benjamin Paz
   and Dr. Eleana Vargas de Nieto for providing laboratory research space
   and support at the Universidad Nacional de San Agustin located in
   Arequipa, Peru; Antonio Ballon and Nicanor their help in the collection
   of samples; Ryan Callegan and Danielle Bagaley for their help in working
   out the sensitivity equation; Dr. Jean Jordan for provision of initial
   supplies of primers; Cepheid, Inc., for the loan of a Smart Cycler for
   the field work; Fred Rainey for help in developing initial field
   deployment protocols; and two anonymous reviewers for many constructive
   and helpful ideas for improving this manuscript. Acknowledgement is
   given to the NASA ASTEP program for providing partial funds in support
   of this research work.
NR 38
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U1 3
U2 22
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA
SN 0008-4166
J9 CAN J MICROBIOL
JI Can. J. Microbiol.
PD NOV
PY 2011
VL 57
IS 11
BP 953
EP 963
DI 10.1139/W11-091
PG 11
WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology;
   Immunology; Microbiology
SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology;
   Immunology; Microbiology
GA 861JS
UT WOS:000298015800010
PM 22035208
ER

PT J
AU Li, W
   Yang, C
   Nebert, D
   Raskin, R
   Houser, P
   Wu, H
   Li, Z
AF Li, W.
   Yang, C.
   Nebert, D.
   Raskin, R.
   Houser, P.
   Wu, H.
   Li, Z.
TI Semantic-based web service discovery and chaining for building an Arctic
   spatial data infrastructure
SO COMPUTERS & GEOSCIENCES
LA English
DT Article
DE SDI; Hydrology; Arctic; Ontology; Crawler; Semantic; Service chain;
   Knowledge base
ID SNOW COVER; CYBERINFRASTRUCTURE; CLIMATE; FUTURE
AB Increasing interests in a global environment and climate change have led to studies focused on the changes in the multinational Arctic region. To facilitate Arctic research, a spatial data infrastructure (SDI), where Arctic data, information, and services are shared and integrated in a seamless manner, particularly in light of today's climate change scenarios, is urgently needed. In this paper, we utilize the knowledge-based approach and the spatial web portal technology to prototype an Arctic SDI (ASDI) by proposing (1) a hybrid approach for efficient service discovery from distributed web catalogs and the dynamic Internet: (2) a domain knowledge base to model the latent semantic relationships among scientific data and services: and (3) an intelligent logic reasoning mechanism for (semi-)automatic service selection and chaining. A study of the influence of solid water dynamics to the bio-habitat of the Arctic region is used as an example to demonstrate the prototype. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Li, W.; Yang, C.; Houser, P.; Wu, H.; Li, Z.] George Mason Univ, Dept Geog & GeoInformat Sci, Fairfax, VA 22030 USA.
   [Nebert, D.] Fed Geog Data Comm, Reston, VA 20192 USA.
   [Raskin, R.] NASA, Jet Prop Lab, Pasadena, CA USA.
RP Li, W (reprint author), George Mason Univ, Dept Geog & GeoInformat Sci, Fairfax, VA 22030 USA.
EM wli6@gmu.edu; cyang3@gmu.edu
RI Houser, Paul/J-9515-2013; Yang, Chaowei/A-9881-2017; 
OI Houser, Paul/0000-0002-2991-0441; Yang, Chaowei/0000-0001-7768-4066
NR 76
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U1 2
U2 21
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD NOV
PY 2011
VL 37
IS 11
BP 1752
EP 1762
DI 10.1016/j.cageo.2011.06.024
PG 11
WC Computer Science, Interdisciplinary Applications; Geosciences,
   Multidisciplinary
SC Computer Science; Geology
GA 876WZ
UT WOS:000299139800005
ER

PT J
AU Schmerr, N
   Thomas, C
AF Schmerr, Nicholas
   Thomas, Christine
TI Subducted lithosphere beneath the Kuriles from migration of PP
   precursors
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Kurile Subduction Zone; upper mantle; discontinuities; PP precursors;
   P660P; transition zone
ID MANTLE TRANSITION ZONE; 660 KM DISCONTINUITY; EARTHS MANTLE; SS
   PRECURSORS; SEISMIC DISCONTINUITY; PHASE-TRANSITIONS; SYSTEM
   MG2SIO4-FE2SIO4; NORTHWEST PACIFIC; SLAB PENETRATION; HIGH-PRESSURES
AB We seismically image both thermal and chemical heterogeneity of the mantle beneath the Kurile subduction zone using P-wave energy reflected from the underside of discontinuities, arriving as precursors to the seismic phase PP. We take advantage of new broadband seismic data provided by the High Lava Plains Seismic Experiment and EarthScope's USArray, collecting a dataset of 31 high-quality Sumatran earthquakes sampling beneath the Kuriles. We employ high-resolution array analysis techniques, including migration and vespagrams, to identify precursory arrivals and study lateral variations in discontinuity depth, sharpness, and impedance of the mantle transition zone. We find the 410 km boundary is at 395 km near the subducting Kurile slab, though the boundary is 410-425 km deep elsewhere. In regions away from subduction, we do not detect a laterally continuous underside reflection of P-waves from the 660 km discontinuity. However, in the vicinity of the subducting Kurile slab, we detect robust P660P reflections from interfaces near 620-670 km depth, signifying an increase in the impedance contrast at 660 km depth. We also detect deeper reflectors, down to 720 km depth, beneath the Kurile slab in a localized area. Cold, aluminum-depleted harzburgitic lithosphere residing at the base of the transition zone best explains the local enhancement of the 660 km discontinuity P-wave impedance contrast. Our new discontinuity measurements support the hypothesis of cold, depleted lithosphere stagnating at the 660 km discontinuity beneath the Kuriles subduction zone, and imply the 660 km boundary can locally impede mantle flow and produce chemical heterogeneity within the transition zone. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Schmerr, Nicholas] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
   [Thomas, Christine] Univ Munster, Inst Geophys, D-48149 Munster, Germany.
RP Schmerr, N (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA.
EM nschmerr@dtm.ciw.edu; tine@earth.uni-muenster.de
RI Schmerr, Nicholas/D-7338-2012; 
OI Schmerr, Nicholas/0000-0002-3256-1262
FU National Science Foundation; GEO Directorate through National Science
   Foundation; Department of Terrestrial Magnetism Postdoctoral Fellowship;
    [DFG1530/2-1]
FX We are grateful for the constructive comments and suggestions provided
   by the editor Peter Shearer and two anonymous reviewers that helped to
   greatly improve the quality of the manuscript. Data were collected with
   the Standing Order for Data (Owens et al., 2004) software. We thank the
   HLP project for providing access to their data. Data from the TA network
   were made freely available as part of the EarthScope USArray facility
   supported by the National Science Foundation. The facilities of the IRIS
   Data Management System, and specifically the IRIS Data Management
   Center, were used for access to waveform, metadata or products required
   in this study. The IRIS-DMS is funded through the National Science
   Foundation and specifically the GEO Directorate through the
   Instrumentation and Facilities Program of the National Science
   Foundation. Data analyses were performed with the TauP (Crotwell et al.,
   1999), Seismic Handler (Stammler, 1993), and Seismic Analysis Code
   (Goldstein et al., 2003) toolkits. Figures were generated using GMT
   (Wessel and Smith, 1998). N.S. was supported by a Department of
   Terrestrial Magnetism Postdoctoral Fellowship, and C. T. was supported
   under grant DFG1530/2-1.
NR 85
TC 15
Z9 17
U1 1
U2 21
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD NOV 1
PY 2011
VL 311
IS 1-2
BP 101
EP 111
DI 10.1016/j.epsl.2011.09.002
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 864WB
UT WOS:000298270100009
ER

PT J
AU Gubitosi, G
   Migliaccio, M
   Pagano, L
   Amelino-Camelia, G
   Melchiorri, A
   Natoli, P
   Polenta, G
AF Gubitosi, Giulia
   Migliaccio, Marina
   Pagano, Luca
   Amelino-Camelia, Giovanni
   Melchiorri, Alessandro
   Natoli, Paolo
   Polenta, Gianluca
TI Using CMB data to constrain non-isotropic Planck-scale modifications to
   Electrodynamics
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE CMBR polarisation; cosmological parameters from CMBR; quantum gravity
   phenomenology; CMBR theory
ID PROBE WMAP OBSERVATIONS; QUANTUM-GRAVITY; VIOLATION; LIMITS
AB We develop a method to constrain non-isotropic features of Cosmic Microwave Background (CMB) polarization, of a type expected to arise in some models describing quantum gravity effects on light propagation. We describe the expected signatures of this kind of anmalous light propagation on CMB photons, showing that it will produce a non-isotropic birefringence effect, i.e. a rotation of the CMB polarization direction whose observed amount depends in a peculiar way on the observation direction. We also show that the sensitivity levels expected for CMB polarization studies by the Planck satellite are sufficient for testing these effects if, as assumed in the quantum-gravity literature, their magnitude is set by the minute Planck length.
C1 [Gubitosi, Giulia] Berkeley Lab, Berkeley, CA 94720 USA.
   [Gubitosi, Giulia] Univ Calif Berkeley, Berkeley, CA 94720 USA.
   [Migliaccio, Marina] Univ Roma Tor Vergata, Rome, Italy.
   [Pagano, Luca] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Amelino-Camelia, Giovanni; Melchiorri, Alessandro] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
   Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy.
   [Natoli, Paolo] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy.
   INAF IASF Bologna, Bologna, Italy.
   [Natoli, Paolo; Polenta, Gianluca] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
   [Polenta, Gianluca] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
RP Gubitosi, G (reprint author), Berkeley Lab, Berkeley, CA 94720 USA.
EM giulia.gubitosi@berkeley.edu; Marina.Migliaccio@roma2.infn.it;
   luca.pagano@jpl.nasa.gov; giovanni.amelino-camelia@roma1.infn.it;
   alessandro.melchiorri@roma1.infn.it; paolo.natoli@roma2.infn.it;
   gianluca.polenta@asdc.asi.it
RI Gubitosi, Giulia/J-3142-2012; 
OI Polenta, Gianluca/0000-0003-4067-9196; Melchiorri,
   Alessandro/0000-0001-5326-6003; Gubitosi, Giulia/0000-0001-6107-639X
FU National Aeronautics and Space Administration; PRIN-INAF; Italian Space
   Agency through the ASI [Euclid-IC (I/031/10/0)]; DOE
   [DE-AC03-76SF00098]; CASPER (Rome, Italy); ASI
FX Part of the research of was carried out at the Jet Propulsion
   Laboratory. California Institute of Technology, under a contract with
   the National Aeronautics and Space Administration.; This work is
   supported by PRIN-INAF, "Astronomy probes fundamental physics". Support
   was given by the Italian Space Agency through the ASI contracts
   Euclid-IC (I/031/10/0).; This research used resources at NERSC,
   supported by the DOE under Contract No. DE-AC03-76SF00098, and at CASPER
   (Rome, Italy: special thanks are due to NI. Botti and F. Massaioli).; We
   also acknowledge support from ASI Contract Planck LFI activity of Phase
   E2.
NR 32
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD NOV
PY 2011
IS 11
AR 003
DI 10.1088/1475-7516/2011/11/003
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 863CV
UT WOS:000298141300003
ER

PT J
AU Handschuh, RF
   Zakrajsek, AJ
AF Handschuh, Robert F.
   Zakrajsek, Andrew J.
TI High-Pressure Angle Gears: Comparison to Typical Gear Designs
SO JOURNAL OF MECHANICAL DESIGN
LA English
DT Article
AB A preliminary study has been completed to determine the feasibility of using high-pressure angle gears in aeronautic and space applications. Tests were conducted in the NASA GRC Spur Gear Test Facility at speeds up to 10,000 rpm and 73 N m (648 in. lb) for 3.18, 2.12, and 1.59 module gears (8, 12, and 16 diametral pitch gears), all designed to operate in the same test facility. The 3.18 module (8-diametral pitch), 28 tooth, 20 deg pressure angle gears are the NASA GRC baseline test specimen. Also, 2.12 module (12-diametral pitch), 42 tooth, 25 deg pressure angle gears were tested. Finally, 1.59 module (16-diametral pitch), 56 tooth, 35 deg pressure angle gears were tested. The high-pressure angle gears were the most efficient when operated in the high-speed aerospace mode (10,000 rpm, lubricated with a synthetic turbine engine oil) and produced the lowest wear rates when tested with a perfluoroether-based grease. The grease tests were conducted at 150 rpm and 71 N m (630 in. lb). [DOI:10.1115/1.4004458]
C1 [Handschuh, Robert F.; Zakrajsek, Andrew J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Handschuh, RF (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM robert.f.handschuh@nasa.gov; azakrajs@gmail.com
NR 11
TC 2
Z9 2
U1 1
U2 2
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 1050-0472
J9 J MECH DESIGN
JI J. Mech. Des.
PD NOV
PY 2011
VL 133
IS 11
AR 114501
DI 10.1115/1.4004458
PG 6
WC Engineering, Mechanical
SC Engineering
GA 861HC
UT WOS:000298009000014
ER

PT J
AU Palumbo, D
   Klos, J
AF Palumbo, Dan
   Klos, Jacob
TI The effects of voids and recesses on the transmission loss of honeycomb
   sandwich panels
SO NOISE CONTROL ENGINEERING JOURNAL
LA English
DT Article
AB Sandwich honeycomb composite panels are lightweight and strong, and, therefore, provide a reasonable alternative to the aluminum ring frame/stringer architecture currently used for most aircraft airframes. One drawback to honeycomb panels is that they radiate noise into the aircraft cabin very efficiently provoking the need for additional sound treatment which adds weight and reduces the material's cost advantage. A series of honeycomb panels was made which incorporated different design strategies aimed at reducing the honeycomb panels' radiation efficiency while at the same time maintaining their strength. The majority of the designs were centered on the concept of creating areas of reduced stiffness in the panel by adding voids and recesses to the core. The effort culminated with a reinforced/recessed panel which had 6 dB higher transmission loss than the baseline solid core panel while maintaining comparable strength. (C) 2011 Institute of Noise Control Engineering.
C1 [Palumbo, Dan; Klos, Jacob] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Palumbo, D (reprint author), NASA Langley Res Ctr, MS 463, Hampton, VA 23681 USA.
EM d.l.palumbo@nasa.gov; j.klos@nasa.gov
NR 13
TC 2
Z9 3
U1 2
U2 5
PU INST NOISE CONTROL ENGINEERING
PI AMES
PA IOWA STATE UNIV, COLLEGE ENGINEERING, 212 MARSTON HALL, AMES, IA
   50011-2152 USA
SN 0736-2501
J9 NOISE CONTROL ENG J
JI Noise Control Eng. J.
PD NOV
PY 2011
VL 59
IS 6
BP 631
EP 640
PG 10
WC Acoustics; Engineering, Multidisciplinary
SC Acoustics; Engineering
GA 865YY
UT WOS:000298348000007
ER

PT J
AU Rumsey, CL
   Slotnick, JP
   Long, M
   Stuever, RA
   Wayman, TR
AF Rumsey, C. L.
   Slotnick, J. P.
   Long, M.
   Stuever, R. A.
   Wayman, T. R.
TI Summary of the First AIAA CFD High-Lift Prediction Workshop
SO JOURNAL OF AIRCRAFT
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
AB The first AIAA CFD High-Lift Prediction Workshop was held in Chicago, Illinois, in June 2010. The goals of the workshop included an assessment of the numerical prediction capability of current-generation computational fluid dynamics (CFD) technology/codes for swept, medium/high-aspect-ratio wings in landing/takeoff (high-lift) configurations. Twenty-one participants from eight countries and 18 organizations submitted a total of 39 data sets of CFD results. A variety of grid systems (both structured and unstructured) were used. Trends due to flap angle were analyzed, and effects of grid family, grid density, solver, and turbulence model were addressed. Some participants also assessed the effects of support brackets used to attach the flap and slat to the main wing. This paper analyzes the combined results from all workshop participants. Comparisons with experimental data are made. A statistical summary of the CFD results is also included.
C1 [Rumsey, C. L.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
   [Slotnick, J. P.] Boeing Co, Computat Sci, Huntington Beach, CA 92647 USA.
   [Long, M.] Univ Wyoming, Laramie, WY 82072 USA.
   [Stuever, R. A.] Hawker Beechcraft Corp, Govt Business, Wichita, KS 67201 USA.
   [Wayman, T. R.] Gulfstream Aerosp Corp, Aerodynam, Savannah, GA 31402 USA.
RP Rumsey, CL (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Mail Stop 128, Hampton, VA 23681 USA.
EM C.L.Rumsey@nasa.gov
NR 12
TC 21
Z9 26
U1 0
U2 4
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD NOV-DEC
PY 2011
VL 48
IS 6
BP 2068
EP 2079
DI 10.2514/1.C031447
PG 12
WC Engineering, Aerospace
SC Engineering
GA 860SE
UT WOS:000297967200027
ER

PT J
AU Pak, CG
AF Pak, Chan-gi
TI Unsteady Aerodynamic Model Tuning for Precise Flutter Prediction
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID BANG-BIG-CRUNCH; OPTIMIZATION
C1 NASA, Dryden Flight Res Ctr, Struct Dynam Grp, Aerostruct Branch, Edwards AFB, CA 93523 USA.
RP Pak, CG (reprint author), NASA, Dryden Flight Res Ctr, Struct Dynam Grp, Aerostruct Branch, POB 273, Edwards AFB, CA 93523 USA.
NR 17
TC 3
Z9 3
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD NOV-DEC
PY 2011
VL 48
IS 6
BP 2178
EP 2184
DI 10.2514/1.C031495
PG 7
WC Engineering, Aerospace
SC Engineering
GA 860SE
UT WOS:000297967200041
ER

PT J
AU Nayagam, V
   Williams, FA
AF Nayagam, Vedha
   Williams, F. A.
TI Analysis of the melt phase of a rotating polymer disc supporting a
   diffusion flame
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE laminar reacting flows; solidification/melting
ID KARMAN SWIRLING FLOWS; EXTINCTION
AB When a laminar diffusion flame is established over a spinning, thermoplastic, polymer fuel disc in a quiescent, oxidizing environment, the polymer melts and flows radially outwards, causing some fuel to be lost and not transported to the diffusion flame. The viscosity of the liquid in the melt layer retards the radial flow, thereby determining the amount of fuel lost. The melt layer is analysed here for two limiting cases, namely one in which the liquid viscosity depends strongly on temperature, leading to an asymptotic analysis involving two zones in the liquid, and one in which the liquid viscosity is constant, independent of temperature, so that there is only one zone in the liquid. The utility of these two limits is assessed by comparing their predictions with those of full numerical integrations for poly(methyl methacrylate) (PMMA) discs burning in air at atmospheric pressure.
C1 [Nayagam, Vedha] NASA Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
   [Williams, F. A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA.
RP Nayagam, V (reprint author), NASA Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
EM v.nayagam@grc.nasa.gov
FU NASA Glenn Research Center
FX This work was supported by the Fire Prevention, Detection, and
   Suppression Project at the NASA Glenn Research Center and directed by Dr
   G. Ruff.
NR 17
TC 0
Z9 0
U1 0
U2 2
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-1120
J9 J FLUID MECH
JI J. Fluid Mech.
PD NOV
PY 2011
VL 687
BP 238
EP 253
DI 10.1017/jfm.2011.349
PG 16
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 860EA
UT WOS:000297930400009
ER

PT J
AU Rybin, A
   Chibisova, M
   Webley, P
   Steensen, T
   Izbekov, P
   Neal, C
   Realmuto, V
AF Rybin, Alexander
   Chibisova, Marina
   Webley, Peter
   Steensen, Torge
   Izbekov, Pavel
   Neal, Christina
   Realmuto, Vince
TI Satellite and ground observations of the June 2009 eruption of Sarychev
   Peak volcano, Matua Island, Central Kuriles
SO BULLETIN OF VOLCANOLOGY
LA English
DT Article
DE Sarychev Peak; Kurile Islands; Remote sensing; Petrology; SVERT;
   Volcanic ash; Sulfur dioxide
ID RESOLUTION-IMAGING-SPECTRORADIOMETER; SULFUR-DIOXIDE EMISSIONS; KILAUEA
   VOLCANO; ASH CLOUDS; TRANSPORT; ALASKA; SO2; RETRIEVAL; FAILURES; HAWAII
AB After 33 years of repose, one of the most active volcanoes of the Kurile island arc-Sarychev Peak on Matua Island in the Central Kuriles-erupted violently on June 11, 2009. The eruption lasted 9 days and stands among the largest of recent historical eruptions in the Kurile Island chain. Satellite monitoring of the eruption, using Moderate Resolution Imaging Spectroradiometer, Meteorological Agency Multifunctional Transport Satellite, and Advanced Very High Resolution Radiometer data, indicated at least 23 separate explosions between 11 and 16 June 2009. Eruptive clouds reached altitudes of generally 8-16 km above sea level (ASL) and in some cases up to 21 km asl. Clouds of volcanic ash and gas stretched to the north and northwest up to 1,500 km and to the southeast for more than 3,000 km. For the first time in recorded history, ash fall occurred on Sakhalin Island and in the northeast sector of the Khabarovsky Region, Russia. Based on satellite image analysis and reconnaissance field studies in the summer of 2009, the eruption produced explosive tephra deposits with an estimated bulk volume of 0.4 km(3). The eruption is considered to have a Volcanic Explosivity Index of 4. Because the volcano is remote, there was minimal risk to people or infrastructure on the ground. Aviation transport, however, was significantly disrupted because of the proximity of air routes to the volcano.
C1 [Webley, Peter; Steensen, Torge; Izbekov, Pavel] Univ Alaska Fairbanks, Inst Geophys, Alaska Volcano Observ, Fairbanks, AK 99775 USA.
   [Rybin, Alexander; Chibisova, Marina] Sakhalin Volcan Erupt Response Team, Inst Marine Geol & Geophys, Yuzhno Sakhalinsk 693022, Russia.
   [Neal, Christina] US Geol Survey, Alaska Volcano Observ, Anchorage, AK 99508 USA.
   [Realmuto, Vince] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Webley, P (reprint author), Univ Alaska Fairbanks, Inst Geophys, Alaska Volcano Observ, 903 Koyukuk Dr, Fairbanks, AK 99775 USA.
EM pwebley@gi.alaska.edu
RI Izbekov, Pavel/B-5110-2010; Webley, Peter/F-8238-2015
OI Webley, Peter/0000-0001-5327-8151
NR 59
TC 22
Z9 23
U1 1
U2 16
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0258-8900
J9 B VOLCANOL
JI Bull. Volcanol.
PD NOV
PY 2011
VL 73
IS 9
BP 1377
EP 1392
DI 10.1007/s00445-011-0481-0
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA 857RT
UT WOS:000297737100020
ER

PT J
AU Holzmann, GJ
   Joshi, R
   Groce, A
AF Holzmann, Gerard J.
   Joshi, Rajeev
   Groce, Alex
TI Swarm Verification Techniques
SO IEEE TRANSACTIONS ON SOFTWARE ENGINEERING
LA English
DT Article
DE Software engineering tools and techniques; logic model checking;
   distributed algorithms; software verification
AB The range of verification problems that can be solved with logic model checking tools has increased significantly in the last few decades. This increase in capability is based on algorithmic advances and new theoretical insights, but it has also benefitted from the steady increase in processing speeds and main memory sizes on standard computers. The steady increase in processing speeds, though, ended when chip-makers started redirecting their efforts to the development of multicore systems. For the near-term future, we can anticipate the appearance of systems with large numbers of CPU cores, but without matching increases in clock-speeds. We will describe a model checking strategy that can allow us to leverage this trend and that allows us to tackle significantly larger problem sizes than before.
C1 [Holzmann, Gerard J.; Joshi, Rajeev] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
   [Groce, Alex] Oregon State Univ, Sch Elect Engn & Comp Sci, Kelley Engn Ctr 1148, Corvallis, OR 97331 USA.
RP Holzmann, GJ (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gerard.holzmann@jpl.nasa.gov; rajeev.joshi@jpl.nasa.gov;
   agroce@gmail.com
FU US National Aeronautics and Space Administration (NASA)
FX The research described in this paper was carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the US National Aeronautics and Space Administration
   (NASA). The work was supported in part by NASA's Exploration Technology
   Development Program (ETDP) on Reliable Software Engineering.
NR 22
TC 20
Z9 20
U1 0
U2 3
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0098-5589
J9 IEEE T SOFTWARE ENG
JI IEEE Trans. Softw. Eng.
PD NOV-DEC
PY 2011
VL 37
IS 6
BP 845
EP 857
DI 10.1109/TSE.2010.110
PG 13
WC Computer Science, Software Engineering; Engineering, Electrical &
   Electronic
SC Computer Science; Engineering
GA 854SE
UT WOS:000297513700006
ER

PT J
AU Jacobson, AR
   Holzworth, RH
   McCarthy, MP
   Pfaff, RF
AF Jacobson, Abram R.
   Holzworth, Robert H.
   McCarthy, Michael P.
   Pfaff, Robert F.
TI Initial Studies with the Lightning Detector on the C/NOFS Satellite, and
   Cross Validation with WWLLN
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID OPTICAL TRANSIENT DETECTOR; LOCATION NETWORK WWLLN; PHOTODIODE DETECTOR;
   FORTE SATELLITE; ICE-SCATTERING; FREQUENCY; TROPICS; TRMM; ACCURACY;
   RAINFALL
AB The lightning detector (LD) on the Communications/Navigation Outage Forecast System (C/NOFS) satellite uses a pair of silicon photodiodes, viewing each flank at right angles to the satellite track over an extended field of view. The data product is a report every 1/2 s of the number of digitizer cycles (125 mu s each) for which the detected power was in predefined ranges. The performance of this system over the first 2.5 years of the C/NOFS mission is discussed, statistics of its lightning observations are presented, and a statistical cross validation using the World-Wide Lightning Location Network (WWLLN) as a ground truth is provided. It is found that the LD reports of lightning, despite their blunt timing (1/2 s), show correlation with strokes detected and located by WWLLN. The irradiance of these strokes lies on the high-power flank of the irradiance distribution seen earlier by the FORTE satellite. Thus, the LD thresholds favor high-power lightning; it is shown that the closest portion of the field of view is more likely to provide WWLLN coincidences than is the furthest portion of the field of view. Statistics of lightning incidence are examined at low latitudes, versus longitude, and distributions that are consistent with those established earlier by the OTD and LIS instruments are retrieved. Finally, the longitude dependence of the irradiance per stroke is examined and the ways in which it differs between the three major lightning "hot spots" is explored. It is observed that the radiance per stroke over the Congo Basin is lower than that over the other two hot spots (Maritime Continent/South Asia and the Americas), consistent with earlier observations by the OTD imager.
C1 [Jacobson, Abram R.; Holzworth, Robert H.; McCarthy, Michael P.] Univ Washington, Seattle, WA 98195 USA.
   [Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA.
RP Jacobson, AR (reprint author), Univ Washington, Box 351310, Seattle, WA 98195 USA.
EM abramj@u.washington.edu
RI Pfaff, Robert/F-5703-2012
OI Pfaff, Robert/0000-0002-4881-9715
FU Air Force Research Laboratory; Department of Defense; National
   Aeronautics and Space Administration (NASA) [NNX08AD12G]; Naval Research
   Laboratory; Aerospace Corporation; AFOSR [FA9550-09-1-0309]; Defense
   Advanced Research Agency
FX The C/NOFS mission is supported by the Air Force Research Laboratory,
   the Department of Defense Space Test Program, the National Aeronautics
   and Space Administration (NASA), the Naval Research Laboratory, and the
   Aerospace Corporation. This analysis at the University of Washington was
   supported in part by AFOSR Grant FA9550-09-1-0309, in part by NASA Grant
   NNX08AD12G, and by the Defense Advanced Research Agency's Nimbus
   program. The authors wish to thank the World Wide Lightning Location
   Network (http://wwlln.net), a collaboration among over 40 universities
   and institutions, for providing the lightning location data used in this
   paper.
NR 37
TC 2
Z9 2
U1 1
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD NOV
PY 2011
VL 28
IS 11
BP 1423
EP 1435
DI 10.1175/JTECH-D-11-00047.1
PG 13
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 854HD
UT WOS:000297484700005
ER

PT J
AU He, ZH
   Zhang, Y
   Mehta, SK
   Pierson, DL
   Wu, HL
   Rohde, LH
AF He, Zhenhua
   Zhang, Ye
   Mehta, Satish K.
   Pierson, Duane L.
   Wu, Honglu
   Rohde, Larry H.
TI Expression Profile of Apoptosis Related Genes and Radio-sensitivity of
   Prostate Cancer Cells
SO JOURNAL OF RADIATION RESEARCH
LA English
DT Article
DE Prostate cancer cells; X-rays; Monensin; Apoptosis; Gene expression
ID MEDIATED GROWTH-INHIBITION; STAUROSPORINE-INDUCED APOPTOSIS; CYCLE
   ARREST; CARCINOMA-CELLS; DIFFERENTIAL EXPRESSION; SIGNALING PATHWAYS;
   LEUKEMIA-CELLS; PC-3 CELLS; MONENSIN; LINES
AB Radio-resistant or recurrent prostate cancer represents a serious health risk for approximately 20%-30% of patients treated with primary radiation therapy for clinically localized prostate cancer. In the present study, we investigated the expression profiles of 84 genes involved in various apoptosis pathways in two prostate cancer cell lines LNCaP (P53+ and AR+) and PC3 (P53- and AR-). We also studied the effect of monensin, an apoptosis inducing reagent, in X-ray-induced cell killing. Comparison of gene expressions between unirradiated LNCaP and PC3 cells revealed distinguished gene expression patterns. The data showed a significantly higher expression level of genes involved in the caspase/card family and the TNF ligand/receptor family in PC3 cells, whereas, LNCaP cells exhibited higher expressions in the p53 related genes. At 2 and 4 hrs post a 10 Gy X-ray exposure, changes of gene expressions were detected in a significant fraction of the genes in LNCaP cells, but no significant changes were found in PC3 cells. There was no significant apoptosis-inducing effect of X-rays (up to 10 Gy) in both cell lines; however, monensin was shown to be effective in inducing apoptosis in LNCaP, but not in PC3 cells. In addition, the effect of combined treatment of monensin and X-rays in LNCaP cells appeared to be synergistic. Our results suggest that monensin may be effective for both cancer cell killing and radiosensitizing, and the different expression profiles in apoptosis related genes in cancer cells may be correlated with their sensitivity to apoptosis inducing reagents.
C1 [Zhang, Ye] Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA.
   [He, Zhenhua] Lanzhou Univ, Lanzhou 730000, Gansu, Peoples R China.
   [He, Zhenhua; Rohde, Larry H.] Univ Houston Clear Lake City, Houston, TX 77058 USA.
   [Zhang, Ye; Mehta, Satish K.; Pierson, Duane L.; Wu, Honglu] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
   [Mehta, Satish K.] Enterprise Advisory Serv Inc, Houston, TX 77058 USA.
RP Zhang, Y (reprint author), Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA.
EM ye.zhang-1@nasa.gov
FU University of Houston, Institute for Space Systems Operations (ISSO)
FX This work was supported in part by the University of Houston, Institute
   for Space Systems Operations (ISSO) Post-Doctoral Aerospace Fellowship
   Program. We would like to thank Prof. Yirong Chen for his constructive
   comments on this project. Dr. Ye Zhang was employed by University of
   Houston at Clear Lake while the work was performed.
NR 43
TC 8
Z9 10
U1 0
U2 3
PU JAPAN RADIATION RESEARCH SOC
PI CHIBA
PA C/O NAT INST RADIOLOGICAL SCI 9-1 ANAGAWA-4-CHOME INAGE-KU, CHIBA, 263,
   JAPAN
SN 0449-3060
J9 J RADIAT RES
JI J. Radiat. Res.
PD NOV
PY 2011
VL 52
IS 6
BP 743
EP 751
DI 10.1269/jrr.10190
PG 9
WC Biology; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Radiology, Nuclear Medicine
   & Medical Imaging
GA 855LL
UT WOS:000297565800008
PM 22020081
ER

PT J
AU Simpson, HJ
   Collis, JM
   Soukup, RJ
   Collins, MD
   Siegmann, WL
AF Simpson, Harry J.
   Collis, Jon M.
   Soukup, Raymond J.
   Collins, Michael D.
   Siegmann, William L.
TI Experimental testing of the variable rotated elastic parabolic equation
SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA
LA English
DT Article
ID PROPAGATION; INTERFACE
AB A series of laboratory experiments was conducted to obtain high-quality data for acoustic propagation in shallow water waveguides with sloping elastic bottoms. Accurate modeling of transmission loss in these waveguides can be performed with the variable rotated parabolic equation method. Results from an earlier experiment with a flat or sloped slab of polyvinyl chloride (PVC) demonstrated the necessity of accounting for elasticity in the bottom and the ability of the model to produce benchmark-quality agreement with experimental data [J. M. Collis at al., J. Acoust. Soc. Am. 122, 1987-1993 (2007)]. This paper presents results of a second experiment, using two PVC slabs joined at an angle to create a waveguide with variable bottom slope. Acoustic transmissions over the 100-300 kHz band were received on synthetic horizontal arrays for two source positions. The PVC slabs were oriented to produce three different simulated waveguides: flat bottom followed by downslope, upslope followed by flat bottom, and upslope followed by downslope. Parabolic equation solutions for treating variable slopes are benchmarked against the data. [DOI: 10.1121/1.3641415]
C1 [Simpson, Harry J.] USN, Res Lab, Phys Acoust Branch Code 7136, Washington, DC 20375 USA.
   [Collis, Jon M.] Colorado Sch Mines, Dept Appl Math & Stat, Golden, CO 80401 USA.
   [Soukup, Raymond J.] USN, Res Lab, Acoust Div Code 7144, Washington, DC 20375 USA.
   [Collins, Michael D.] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
   [Siegmann, William L.] Rensselaer Polytech Inst, Dept Math Sci, Jonsson Rowland Sci Ctr 1C08, Troy, NY 12180 USA.
RP Simpson, HJ (reprint author), USN, Res Lab, Phys Acoust Branch Code 7136, 4555 Overlook Ave SW, Washington, DC 20375 USA.
EM harry.simpson@nrl.navy.mil
FU Office of Naval Research
FX This work was supported by the Office of Naval Research. J.M.C. was
   partially supported by an ONR Ocean Acoustics Postdoctoral Fellowship
   Grant.
NR 13
TC 3
Z9 3
U1 0
U2 3
PU ACOUSTICAL SOC AMER AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0001-4966
J9 J ACOUST SOC AM
JI J. Acoust. Soc. Am.
PD NOV
PY 2011
VL 130
IS 5
BP 2681
EP 2686
DI 10.1121/1.3641415
PN 1
PG 6
WC Acoustics; Audiology & Speech-Language Pathology
SC Acoustics; Audiology & Speech-Language Pathology
GA 854HV
UT WOS:000297486500025
PM 22087895
ER

PT J
AU Burton, AS
   Glavin, DP
   Callahan, MP
   Dworkin, JP
   Jenniskens, P
   Shaddad, MH
AF Burton, Aaron S.
   Glavin, Daniel P.
   Callahan, Michael P.
   Dworkin, Jason P.
   Jenniskens, Peter
   Shaddad, Muawia H.
TI Heterogeneous distributions of amino acids provide evidence of multiple
   sources within the Almahata Sitta parent body, asteroid 2008 TC3
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID POLYCYCLIC AROMATIC-HYDROCARBONS; MURCHISON METEORITE; ISOTOPE
   COMPOSITION; ORDINARY CHONDRITE; ORGANIC-COMPOUNDS; ENRICHMENT;
   RECOVERY; UREILITE; SAMPLES; BODIES
AB Two new fragments of the Almahata Sitta meteorite and a sample of sand from the related strewn field in the Nubian Desert, Sudan, were analyzed for two to six carbon aliphatic primary amino acids by ultrahigh performance liquid chromatography with UV-fluorescence detection and time-of-flight mass spectrometry (LC-FT/ToF-MS). The distribution of amino acids in fragment #25, an H5 ordinary chondrite, and fragment #27, a polymict ureilite, were compared with results from the previously analyzed fragment #4, also a polymict ureilite. All three meteorite fragments contain 180-270 parts-per-billion (ppb) of amino acids, roughly 1000-fold lower than the total amino acid abundance of the Murchison carbonaceous chondrite. All of the Almahata Sitta fragments analyzed have amino acid distributions that differ from the Nubian Desert sand, which primarily contains L-alpha-amino acids. In addition, the meteorites contain several amino acids that were not detected in the sand, indicating that many of the amino acids are extraterrestrial in origin. Despite their petrological differences, meteorite fragments #25 and #27 contain similar amino acid compositions; however, the distribution of amino acids in fragment #27 was distinct from those in fragment #4, even though both are polymict ureilites from the same parent body. Unlike in CM2 and CR2/3 meteorites, there are low relative abundances of alpha-amino acids in the Almahata Sitta meteorite fragments, which suggest that Strecker-type chemistry was not a significant amino acid formation mechanism. Given the high temperatures that asteroid 2008 TC3 appears to have experienced and lack of evidence for aqueous alteration on the asteroid, it is possible that the extraterrestrial amino acids detected in Almahata Sitta were formed by Fischer-Tropsch/Haber-Bosch type gas-grain reactions at elevated temperatures.
C1 [Burton, Aaron S.; Glavin, Daniel P.; Callahan, Michael P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Jenniskens, Peter] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
   [Shaddad, Muawia H.] Univ Khartoum, Dept Phys, Khartoum 11115, Sudan.
RP Burton, AS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM aaron.s.burton@nasa.gov
RI Callahan, Michael/D-3630-2012; Burton, Aaron/H-2212-2011; Glavin,
   Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012
OI Burton, Aaron/0000-0002-7137-1605; Glavin, Daniel/0000-0001-7779-7765;
   Dworkin, Jason/0000-0002-3961-8997
FU National Aeronautics and Space Administration (NASA) Astrobiology
   Institute; Goddard Center for Astrobiology; NASA
FX We thank the University of Khartoum and the students and staff of the
   Physics and Astronomy Department of the Faculty of Sciences for their
   efforts to recover the meteorites from the Nubian Desert; A. Lewis for
   optimizing the LC analytical separation conditions at GSFC; J. E. Elsila
   for helpful comments during preparation of the manuscript; and P.
   Ehrenfreund and Z. Martins for helpful criticisms during the review
   process. D. P. G., J. P. D., and M. P. C. acknowledge funding support
   from the National Aeronautics and Space Administration (NASA)
   Astrobiology Institute and the Goddard Center for Astrobiology, and the
   NASA Cosmochemistry Program. A. S. B. also acknowledges support from the
   NASA Postdoctoral Program at the Goddard Space Flight Center,
   administered by Oak Ridge Associated Universities through a contract
   with NASA.
NR 28
TC 15
Z9 15
U1 1
U2 7
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 NOV
PY 2011
VL 46
IS 11
BP 1703
EP 1712
DI 10.1111/j.1945-5100.2011.01257.x
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 853GQ
UT WOS:000297414600007
ER

PT J
AU Hecker, C
   Hook, S
   van der Meijde, M
   Bakker, W
   van der Werff, H
   Wilbrink, H
   van Ruitenbeek, F
   de Smeth, B
   van der Meer, F
AF Hecker, Christoph
   Hook, Simon
   van der Meijde, Mark
   Bakker, Wim
   van der Werff, Harald
   Wilbrink, Henk
   van Ruitenbeek, Frank
   de Smeth, Boudewijn
   van der Meer, Freek
TI Thermal Infrared Spectrometer for Earth Science Remote Sensing
   Applications-Instrument Modifications and Measurement Procedures
SO SENSORS
LA English
DT Article
DE vibrational spectroscopy; thermal infrared; Fourier transform infrared
   spectroscopy; directional hemispherical reflectance; earth science;
   remote sensing
ID EMISSION-SPECTROSCOPY; REFLECTANCE; FELDSPARS; SURFACE; ROCKS
AB In this article we describe a new instrumental setup at the University of Twente Faculty ITC with an optimized processing chain to measure absolute directional-hemispherical reflectance values of typical earth science samples in the 2.5 to 16 mu m range. A Bruker Vertex 70 FTIR spectrometer was chosen as the base instrument. It was modified with an external integrating sphere with a 30 mm sampling port to allow measuring large, inhomogeneous samples and quantitatively compare the laboratory results to airborne and spaceborne remote sensing data. During the processing to directional-hemispherical reflectance values, a background radiation subtraction is performed, removing the effect of radiance not reflected from the sample itself on the detector. This provides more accurate reflectance values for low-reflecting samples. Repeat measurements taken over a 20 month period on a quartz sand standard show that the repeatability of the system is very high, with a standard deviation ranging between 0.001 and 0.006 reflectance units depending on wavelength. This high level of repeatability is achieved even after replacing optical components, re-aligning mirrors and placement of sample port reducers. Absolute reflectance values of measurements taken by the instrument here presented compare very favorably to measurements of other leading laboratories taken on identical sample standards.
C1 [Hecker, Christoph; van der Meijde, Mark; Bakker, Wim; van der Werff, Harald; van Ruitenbeek, Frank; de Smeth, Boudewijn; van der Meer, Freek] Univ Twente, Dept Earth Syst Anal, Fac Geoinformat Sci & Earth Observat ITC, NL-7500 AA Enschede, Netherlands.
   [Hook, Simon] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
   [Wilbrink, Henk; de Smeth, Boudewijn] Univ Twente, GeoSci Lab, Fac Geoinformat Sci & Earth Observat ITC, NL-7500 AA Enschede, Netherlands.
RP Hecker, C (reprint author), Univ Twente, Dept Earth Syst Anal, Fac Geoinformat Sci & Earth Observat ITC, Hengelosestr 99,POB 37, NL-7500 AA Enschede, Netherlands.
EM hecker@itc.nl; simon.j.hook@jpl.nasa.gov; vandermeijde@itc.nl;
   bakker@itc.nl; vdwerff@itc.nl; wilbrink@itc.nl; vanruitenbeek@itc.nl;
   desmeth@itc.nl; vdmeer@itc.nl
RI Hecker, Christoph/D-3891-2009; Van der Meer, F.D./A-4273-2010; van der
   Werff, Harald/D-3886-2009; van Ruitenbeek, Frank/D-4099-2009; Bakker,
   Wim/A-3616-2010; van der Meijde, Mark/D-3883-2009
OI Hecker, Christoph/0000-0001-6802-5042; van der Werff,
   Harald/0000-0002-2871-3913; van Ruitenbeek, Frank/0000-0003-2347-1625;
   van der Meijde, Mark/0000-0002-8762-585X
NR 25
TC 19
Z9 19
U1 2
U2 9
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 1424-8220
J9 SENSORS-BASEL
JI Sensors
PD NOV
PY 2011
VL 11
IS 11
BP 10981
EP 10999
DI 10.3390/s111110981
PG 19
WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation
SC Chemistry; Electrochemistry; Instruments & Instrumentation
GA 857EK
UT WOS:000297698600058
PM 22346683
ER

PT J
AU Takahashi, T
   Suzuki, M
   Nomura, R
   Okuda, Y
   Kamiya, K
   Numazawa, T
   Shirron, P
AF Takahashi, Takuya
   Suzuki, Motoya
   Nomura, Ryuji
   Okuda, Yuichi
   Kamiya, Koji
   Numazawa, Takenori
   Shirron, Peter
TI Surface Waves on Superfluid He-4 Under Reduced Gravity
SO MICROGRAVITY SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Microgravity; Jet plane; Parabolic flight; Superfluid; He-4
AB Superfluid He-4 was produced on a small jet plane for the first time using a small GM-refrigerator to condense the liquid and a scroll pump to get the superfluid by evaporation. The surface wave on superfluid under 0.5g (E), 0.1g (E) and 0.05g (E), together with 2g (E) and 1g (E), was successfully examined by an optical method utilizing parabolic flight. Here, g (E) is the gravitational constant on the ground. Assuming that only the fundamental mode was excited as determined by the sample cell width, the resonance peak in the frequency domain was well reproduced by the gravity wave with corresponding gravity constant.
C1 [Takahashi, Takuya; Suzuki, Motoya; Nomura, Ryuji; Okuda, Yuichi] Tokyo Inst Technol, Dept Condensed Matter Phys, Meguro Ku, Tokyo 1528551, Japan.
   [Kamiya, Koji; Numazawa, Takenori] Natl Inst Mat Sci, Tsukuba, Ibaraki, Japan.
   [Shirron, Peter] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Okuda, Y (reprint author), Tokyo Inst Technol, Dept Condensed Matter Phys, Meguro Ku, 2-12-1 O Okayama, Tokyo 1528551, Japan.
EM okuda@ap.titech.ac.jp
RI Nomura, Ryuji/C-3798-2015
OI Nomura, Ryuji/0000-0002-8730-5960
FU Ground-based Research Program for Space Utilization; JAXA; Tokyo
   Institute of Technology
FX We would like to thank Prof. Takeo Satoh of Tohoku Univ. for his
   encouragement in promoting the present project. This research was
   supported by the "Ground-based Research Program for Space Utilization"
   promoted by JAXA and the Global Center of Excellence Program "Nano-
   science and Quantum Physics" of Tokyo Institute of Technology.
NR 11
TC 3
Z9 3
U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0938-0108
J9 MICROGRAVITY SCI TEC
JI Microgravity Sci. Technol.
PD NOV
PY 2011
VL 23
IS 4
BP 365
EP 372
DI 10.1007/s12217-010-9256-z
PG 8
WC Engineering, Aerospace; Thermodynamics; Mechanics
SC Engineering; Thermodynamics; Mechanics
GA 852MH
UT WOS:000297361600001
ER

PT J
AU Kondrachuk, AV
   Boyle, RD
AF Kondrachuk, Alexander V.
   Boyle, Richard D.
TI The Density Difference of Cupula and Endolymph Changes the Mechanics of
   Semicircular Canals
SO MICROGRAVITY SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Semicircular canals; Cupula; Hypergravity; Artificial gravity;
   Microgravity; Centrifuge
ID POSITIONAL NYSTAGMUS; LINEAR ACCELERATION; SQUIRREL-MONKEY; PRESSURE;
   RESPONSES; DYNAMICS; ALCOHOL; NEURONS
AB A precise balance of cupula and endolymph densities is key to the proper sensing of angular acceleration by the semicircular canals (SC). Estimates show that a density difference of cupula and endolymph (DD) as small as similar to 10 (-aEuro parts per thousand 4) g/cm(3) is sufficient to make the SC sensitive to gravity and centrifugal forces provided they are comparable with gravity. As a result this might cause vestibular disorders. There are conditions under which the DD may even exceed this value. One of them is a change of intra-labyrinth pressure (IP) that may take place during a spaceflight. Here, the effect of DD on SC dynamics is considered using a simplified one-dimensional toroidal mathematical model of a canal for rotation with constant or harmonically oscillating angular velocities. The DD results in: dependence of cupula dynamics on orientation of both the gravity vector relative to the SC plane and the axis of rotation, as well as on the distance between the axis of rotation and the center of SC; shift of the cupula to a new position of equilibrium that depends on both the gravity vector and the parameters of head rotation; and onset of cupula oscillations with multiple frequencies under harmonic stimulation. The DD effect may be important under conditions of artificial gravity where the directions of centrifugal forces, the values of which are comparable with Earth's gravity, the orientations of the axis of rotation of a space station, and the axes of the SCs change during movements of the individuals and their habitat.
C1 [Kondrachuk, Alexander V.] Natl Acad Sci Ukraine, Inst Phys, Dept Theoret Phys, UA-03028 Kiev, Ukraine.
   [Boyle, Richard D.] NASA, BioVIS Ctr, Ames Res Ctr, Mountain View, CA USA.
RP Kondrachuk, AV (reprint author), Natl Acad Sci Ukraine, Inst Phys, Dept Theoret Phys, Prospekt Nauki 46, UA-03028 Kiev, Ukraine.
EM kondr@kondr.kiev.ua
NR 21
TC 0
Z9 0
U1 3
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0938-0108
J9 MICROGRAVITY SCI TEC
JI Microgravity Sci. Technol.
PD NOV
PY 2011
VL 23
IS 4
BP 433
EP 438
DI 10.1007/s12217-011-9265-6
PG 6
WC Engineering, Aerospace; Thermodynamics; Mechanics
SC Engineering; Thermodynamics; Mechanics
GA 852MH
UT WOS:000297361600008
ER

PT J
AU Fahed, R
   Moffat, AFJ
   Zorec, J
   Eversberg, T
   Chene, AN
   Alves, F
   Arnold, W
   Bergmann, T
   Corcoran, MF
   Viegas, NGC
   Dougherty, SM
   Fernando, A
   Fremat, Y
   Carreira, LFG
   Hunger, T
   Knapen, JH
   Leadbeater, R
   Dias, FM
   Martayan, C
   Morel, T
   Pittard, JM
   Pollock, AMT
   Rauw, G
   Reinecke, N
   Ribeiro, J
   Romeo, N
   Sanchez-Gallego, JR
   dos Santos, EM
   Schanne, L
   Stahl, O
   Stober, B
   Stober, B
   Vollmann, K
   Williams, PM
AF Fahed, R.
   Moffat, A. F. J.
   Zorec, J.
   Eversberg, T.
   Chene, A. N.
   Alves, F.
   Arnold, W.
   Bergmann, T.
   Corcoran, M. F.
   Viegas, N. G. Correia
   Dougherty, S. M.
   Fernando, A.
   Fremat, Y.
   Carreira, L. F. Gouveia
   Hunger, T.
   Knapen, J. H.
   Leadbeater, R.
   Dias, F. Marques
   Martayan, C.
   Morel, T.
   Pittard, J. M.
   Pollock, A. M. T.
   Rauw, G.
   Reinecke, N.
   Ribeiro, J.
   Romeo, N.
   Sanchez-Gallego, J. R.
   dos Santos, E. M.
   Schanne, L.
   Stahl, O.
   Stober, Ba
   Stober, Be
   Vollmann, K.
   Williams, P. M.
CA Mons Pro-Am Collaboration
TI Spectroscopy of the archetype colliding-wind binary WR 140 during the
   2009 January periastron passage
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: general; stars: fundamental parameters; stars: winds,
   outflows; stars: Wolf-Rayet
ID WOLF-RAYET STARS; CLASSIFICATION; SPECTRA; WR-140; WC; MODELS; RADIO;
   LINES
AB We present the results from the spectroscopic monitoring of WR 140 (WC7pd + O5.5fc) during its latest periastron passage in 2009 January. The observational campaign consisted of a constructive collaboration between amateur and professional astronomers. It took place at six locations, including Teide Observatory, Observatoire de Haute Provence, Dominion Astrophysical Observatory and Observatoire du Mont Megantic. WR 140 is known as the archetype of colliding-wind binaries and it has a relatively long period (8 yr) and high eccentricity (0.9). We provide updated values for the orbital parameters, new estimates for the WR and O star masses and new constraints on the mass-loss rates and colliding-wind geometry.
C1 [Fahed, R.; Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
   [Fahed, R.; Moffat, A. F. J.] Ctr Rech Astrophys Quebec, Quebec City, PQ, Canada.
   [Zorec, J.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
   [Eversberg, T.] Schnorringen Telescope Sci Inst, Waldbrol, Germany.
   [Chene, A. N.] HIA NRC Canada, Canadian Gemini Off, Victoria, BC V9E 2E7, Canada.
   [Chene, A. N.] Univ Concepcion, Dept Astron, Fac Ciencias Fis & Matemat, Concepcion, Chile.
   [Chene, A. N.] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso, Chile.
   [Corcoran, M. F.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
   [Corcoran, M. F.] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.
   [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
   [Dougherty, S. M.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6J9, Canada.
   [Fremat, Y.] Royal Observ Belgium, B-1180 Brussels, Belgium.
   [Knapen, J. H.; Sanchez-Gallego, J. R.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
   [Knapen, J. H.; Sanchez-Gallego, J. R.] Univ La Laguna, Dept Astrofis, E-38200 San Cristobal la Laguna, Tenerife, Spain.
   [Leadbeater, R.] Three Hills Observ, The Birches CA7 1JF, England.
   [Martayan, C.] European Org Astron Res So Hemisphere, Vitacura, Santiago De Chi, Chile.
   [Morel, T.; Rauw, G.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege 1, Sart Tilman, Belgium.
   [Pittard, J. M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
   [Pollock, A. M. T.] European Space Agcy XMM, Newton Sci Operat Ctr, Villanueva De La Canada 28691, Spain.
   [Williams, P. M.] Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
RP Fahed, R (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ C-V, Montreal, PQ H3C 3J7, Canada.
EM fahed@astro.umontreal.ca
RI dos Santos, Eva/N-6351-2013; 
OI dos Santos, Eva/0000-0002-0474-8863; Pittard, Julian/0000-0003-2244-5070
FU NSERC (Canada); FQRNT (Quebec); Comite Mixto ESO-Gobierno de Chile;
   BASAL/FONDAP; Belspo; Royal Society; Instituto de Astrofisica de
   Canarias (IAC)
FX RF is grateful to the whole Mons team and the other amateur astronomers
   who invested personal time and money in this project and contributed to
   its success. AFJM is grateful to NSERC (Canada) and FQRNT (Quebec) for
   financial assistance. ANC acknowledges support from Comite Mixto
   ESO-Gobierno de Chile and from the BASAL/FONDAP project. TM acknowledges
   financial support from Belspo for contract PRODEX-GAIA DPAC. JMP
   gratefully acknowledges support from the Royal Society. PMW is grateful
   to the Institute for Astronomy for hospitality and continued access to
   the facilities of the Royal Observatory, Edinburgh. We are grateful to
   the Instituto de Astrofisica de Canarias (IAC) and its staff for their
   support of the Mons project. We want to thank Professor Francisco
   Sanchez, Director of the IAC, and Dr Miquel Serra for assistance and the
   generous allotment of telescope time at Mons.
NR 29
TC 20
Z9 20
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 418
IS 1
BP 2
EP 13
DI 10.1111/j.1365-2966.2011.19035.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700034
ER

PT J
AU Dariush, A
   Cortese, L
   Eales, S
   Pascale, E
   Smith, MWL
   Dunne, L
   Dye, S
   Scott, D
   Auld, R
   Baes, M
   Bland-Hawthorn, J
   Buttiglione, S
   Cava, A
   Clements, DL
   Cooray, A
   DeZotti, G
   Driver, S
   Fritz, J
   Gomez, HL
   Hopkins, A
   Hopwood, R
   Ivison, RJ
   Jarvis, MJ
   Jones, DH
   Kelvin, L
   Khosroshahi, HG
   Liske, J
   Loveday, J
   Maddox, S
   Madore, BF
   Michalowski, MJ
   Norberg, P
   Phillipps, S
   Pohlen, M
   Popescu, CC
   Prescott, M
   Rigby, E
   Robotham, A
   Rodighiero, G
   Seibert, M
   Smith, DJB
   Temi, P
   Tuffs, RJ
   van der Werf, PP
AF Dariush, A.
   Cortese, L.
   Eales, S.
   Pascale, E.
   Smith, M. W. L.
   Dunne, L.
   Dye, S.
   Scott, D.
   Auld, R.
   Baes, M.
   Bland-Hawthorn, J.
   Buttiglione, S.
   Cava, A.
   Clements, D. L.
   Cooray, A.
   DeZotti, G.
   Driver, S.
   Fritz, J.
   Gomez, H. L.
   Hopkins, A.
   Hopwood, R.
   Ivison, R. J.
   Jarvis, M. J.
   Jones, D. H.
   Kelvin, L.
   Khosroshahi, H. G.
   Liske, J.
   Loveday, J.
   Maddox, S.
   Madore, B. F.
   Michalowski, M. J.
   Norberg, P.
   Phillipps, S.
   Pohlen, M.
   Popescu, C. C.
   Prescott, M.
   Rigby, E.
   Robotham, A.
   Rodighiero, G.
   Seibert, M.
   Smith, D. J. B.
   Temi, P.
   Tuffs, R. J.
   van der Werf, P. P.
TI The environment and characteristics of low-redshift galaxies detected by
   the Herschel-ATLAS
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; galaxies: general; galaxies: statistics;
   submillimetre: galaxies; submillimetre: general
ID DIGITAL SKY SURVEY; SCIENCE DEMONSTRATION PHASE; VIRGO CLUSTER GALAXIES;
   STAR-FORMATION; DATA RELEASE; LUMINOSITY FUNCTION; DUST ATTENUATION;
   BASIC PROPERTIES; STELLAR MASS; COLD DUST
AB We investigate the ultraviolet and optical properties and environment of low-redshift galaxies detected in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) science demonstration data. We use the Sloan Digital Sky Survey seventh release and the Galaxy And Mass Assembly data base to select galaxies with mag in the redshift range 0.02 = z = 0.2 and look for their submillimetre counterparts in H-ATLAS. Our results show that at low redshift, H-ATLAS detects mainly blue/star-forming galaxies with a minor contribution from red systems which are highly obscured by dust. In addition we find that the colour of a galaxy rather than the local density of its environment determines whether it is detectable by H-ATLAS. The average dust temperature of galaxies that are simultaneously detected by both PACS and SPIRE is 25 +/- 4 K, independent of environment. This analysis provides a glimpse of the potential of the H-ATLAS data to investigate the submillimetre properties of galaxies in the local universe.
C1 [Dariush, A.; Eales, S.; Pascale, E.; Smith, M. W. L.; Dye, S.; Auld, R.; Gomez, H. L.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
   [Dariush, A.; Clements, D. L.; Hopwood, R.] Imperial Coll Sch Med, Dept Phys, London SW7 2AZ, England.
   [Cortese, L.; Liske, J.] European So Observ, D-85748 Garching, Germany.
   [Dunne, L.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
   [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
   [Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
   [Bland-Hawthorn, J.] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia.
   [Buttiglione, S.; DeZotti, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
   [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
   [Cooray, A.] UC Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [DeZotti, G.] SISSA, I-34136 Trieste, Italy.
   [Driver, S.; Kelvin, L.; Robotham, A.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
   [Hopkins, A.] Australian Astron Observ, Epping, NSW 1710, Australia.
   [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Ivison, R. J.; Michalowski, M. J.; Norberg, P.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Jarvis, M. J.; van der Werf, P. P.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
   [Jones, D. H.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
   [Khosroshahi, H. G.] IPM Sch Astron, Tehran, Iran.
   [Loveday, J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
   [Madore, B. F.; Seibert, M.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
   [Phillipps, S.] Univ Bristol, HH Wills Phys Lab, Astrophys Grp, Bristol BS8 1TL, Avon, England.
   [Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
   [Prescott, M.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
   [Rodighiero, G.] Univ Padua, I-35122 Padua, Italy.
   [Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Tuffs, R. J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
   [van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Dariush, A (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
EM a.dariush@imperial.ac.uk
RI Gomez, Haley/C-2800-2009; Baes, Maarten/I-6985-2013; Robotham,
   Aaron/H-5733-2014; Driver, Simon/H-9115-2014; Ivison, R./G-4450-2011;
   Cava, Antonio/C-5274-2017; 
OI Smith, Daniel/0000-0001-9708-253X; Phillipps,
   Steven/0000-0001-5991-3486; Rodighiero, Giulia/0000-0002-9415-2296;
   Liske, Jochen/0000-0001-7542-2927; Cortese, Luca/0000-0002-7422-9823;
   Dye, Simon/0000-0002-1318-8343; Baes, Maarten/0000-0002-3930-2757;
   Robotham, Aaron/0000-0003-0429-3579; Driver, Simon/0000-0001-9491-7327;
   Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275;
   Maddox, Stephen/0000-0001-5549-195X; Scott, Douglas/0000-0002-6878-9840
FU STFC (UK); ARC (Australia); AAO; Alfred P. Sloan Foundation; National
   Science Foundation; US Department of Energy; National Aeronautics and
   Space Administration; Japanese Monbukagakusho; Max Planck Society;
   Higher Education Funding Council for England; American Museum of Natural
   History; Astrophysical Institute Potsdam; University of Basel;
   University of Cambridge; Case Western Reserve University; University of
   Chicago; Drexel University; Fermilab; Institute for Advanced Study;
   Japan Participation Group; Johns Hopkins University; Joint Institute for
   Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
   Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
   Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
   (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
   University; Ohio State University; University of Pittsburgh; University
   of Portsmouth; Princeton University; United States Naval Observatory;
   University of Washington
FX The Herschel-ATLAS is a project with Herschel, which is an ESA space
   observatory with science instruments provided by Europeanled Principal
   Investigator consortia and with important participation from NASA. The
   H-ATLAS website is http://www.h-atlas.org/. GAMA is a joint
   European-Australasian project based around a spectroscopic campaign
   using the Anglo-Australian Telescope. The GAMA input catalogue is based
   on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared
   Deep Sky Survey. Complementary imaging of the GAMA regions is being
   obtained by a number of independent survey programmes including GALEX
   MIS, VST KIDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP,
   providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC
   (Australia), the AAO and the participating institutions. The GAMA
   website is http://www.gama-survey.org/. Funding for the SDSS and SDSS-II
   has been provided by the Alfred P. Sloan Foundation, the Participating
   Institutions, the National Science Foundation, the US Department of
   Energy, the National Aeronautics and Space Administration, the Japanese
   Monbukagakusho, the Max Planck Society, and the Higher Education Funding
   Council for England. The SDSS Web Site is http://www.sdss.org/.; The
   SDSS is managed by the Astrophysical Research Consortium for the
   Participating Institutions. The Participating Institutions are the
   American Museum of Natural History, Astrophysical Institute Potsdam,
   University of Basel, University of Cambridge, Case Western Reserve
   University, University of Chicago, Drexel University, Fermilab, the
   Institute for Advanced Study, the Japan Participation Group, Johns
   Hopkins University, the Joint Institute for Nuclear Astrophysics, the
   Kavli Institute for Particle Astrophysics and Cosmology, the Korean
   Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos
   National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
   Max-Planck-Institute for Astrophysics (MPA), New Mexico State
   University, Ohio State University, University of Pittsburgh, University
   of Portsmouth, Princeton University, the United States Naval
   Observatory, and the University of Washington.
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SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 418
IS 1
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DI 10.1111/j.1365-2966.2011.19340.x
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SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700037
ER

PT J
AU Blomme, J
   Sarro, LM
   O'Donovan, FT
   Debosscher, J
   Brown, T
   Lopez, M
   Dubath, P
   Rimoldini, L
   Charbonneau, D
   Dunham, E
   Mandushev, G
   Ciardi, DR
   De Ridder, J
   Aerts, C
AF Blomme, J.
   Sarro, L. M.
   O'Donovan, F. T.
   Debosscher, J.
   Brown, T.
   Lopez, M.
   Dubath, P.
   Rimoldini, L.
   Charbonneau, D.
   Dunham, E.
   Mandushev, G.
   Ciardi, D. R.
   De Ridder, J.
   Aerts, C.
TI Improved methodology for the automated classification of periodic
   variable stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; methods: statistical; techniques: photometric
ID SUPERVISED CLASSIFICATION
AB We present a novel automated methodology to detect and classify periodic variable stars in a large data base of photometric time series. The methods are based on multivariate Bayesian statistics and use a multistage approach. We applied our method to the ground-based data of the Trans-Atlantic Exoplanet Survey (TrES) Lyr1 field, which is also observed by the Kepler satellite, covering similar to 26 000 stars. We found many eclipsing binaries as well as classical non-radial pulsators, such as slowly pulsating B stars, ? Doradus, beta Cephei and d Scuti stars. Also a few classical radial pulsators were found.
C1 [Blomme, J.; Debosscher, J.; De Ridder, J.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium.
   [Sarro, L. M.] UNED, Dpt Inteligencia Artificial, Madrid 28040, Spain.
   [O'Donovan, F. T.] CALTECH, Pasadena, CA 91125 USA.
   [Brown, T.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
   [Brown, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Lopez, M.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis, E-28691 Villanueva De La Canada, Spain.
   [Dubath, P.; Rimoldini, L.] Observ Geneva, CH-1290 Versoix, Switzerland.
   [Charbonneau, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Dunham, E.; Mandushev, G.] Lowell Observ, Flagstaff, AZ 86001 USA.
   [Ciardi, D. R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Aerts, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegem, Netherlands.
RP Blomme, J (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Heverlee, Belgium.
EM jonas.blomme@ster.kuleuven.be
RI Sarro, Luis/L-8082-2014; O'Donovan, Francis/I-2423-2014; 
OI O'Donovan, Francis/0000-0002-4858-6106; Ciardi,
   David/0000-0002-5741-3047
FU European Research Council under the European Community [227224];
   Research Council of K. U. Leuven [GOA/2008/04]; Fund for Scientific
   Research of Flanders [G.0332.06]; Belgian Federal Science Policy Office
   [C90309, C90291]; Spanish Ministerio de Educacion y Ciencia
   [AYA2005-04286]
FX The research leading to these results has received funding from the
   European Research Council under the European Community's Seventh
   Framework Programme (FP7/2007-2013)/ERC grant agreement no. 227224
   (PROSPERITY), the Research Council of K. U. Leuven (GOA/2008/04), from
   the Fund for Scientific Research of Flanders (G.0332.06), the Belgian
   Federal Science Policy Office (C90309: CoRoT Data Exploitation, C90291
   Gaia-DPAC) and the Spanish Ministerio de Educacion y Ciencia through
   grant AYA2005-04286. Public access to the TrES data was provided to the
   through the NASA Star and Exoplanet Database (NStED,
   http://nsted.ipac.caltech.edu).
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
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GA 848IR
UT WOS:000297045700040
ER

PT J
AU Jurua, E
   Charles, PA
   Still, M
   Meintjes, PJ
AF Jurua, E.
   Charles, P. A.
   Still, M.
   Meintjes, P. J.
TI The optical and X-ray light curves of Hercules X-1
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion; accretion discs; radiation mechanisms: thermal; scattering;
   stars: binaries: close; stars: neutron; stars: pulsars: individual: Her
   X1
ID SHORT HIGH STATE; MAGNETIC NEUTRON-STARS; ANOMALOUS LOW STATE; X-1-HZ
   HERCULIS; HZ-HERCULIS; DISK; MASS; ACCRETION; SUPERWASP; PERIOD
AB The Galactic neutron star X-ray binary Her X-1 displays a well-known 35-day superorbital modulation in its X-ray and optical light curves. Detected across a broad energy range, the modulation is prevalent in X-rays, cycling between low and high states. The 35-day modulation is believed to be the result of the periodic occultation of the neutron star by a warped precessing accretion disc. Using optical observations of Her X-1 during both the anomalous low state (ALS) and the normal high state, it is shown that the orbital light curve of Her X-1 varies systematically over the 35-day precession cycle. The 35-day precessional profile is remarkably consistent between the ALS and normal high state of Her X-1, suggesting only a very slight change in the form of the disc warp between the two states. Comparison of optical and X-ray light curves suggests that a significant component of the X-ray flux during the ALS originates from the companion star.
C1 [Jurua, E.; Meintjes, P. J.] Univ Free State, ZA-9300 Bloemfontein, South Africa.
   [Jurua, E.] Mbarara Univ Sci & Technol, Mbarara, Uganda.
   [Charles, P. A.] S African Astron Observ, ZA-7935 Observatory, South Africa.
   [Charles, P. A.] Univ Cape Town, ZA-7701 Rondebosch, South Africa.
   [Charles, P. A.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
   [Still, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Jurua, E (reprint author), Univ Free State, POB 339, ZA-9300 Bloemfontein, South Africa.
EM ejurua@gmail.com; MeintjPJ@ufs.ac.za
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 418
IS 1
BP 437
EP 443
DI 10.1111/j.1365-2966.2011.19494.x
PG 7
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SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700064
ER

PT J
AU Tombesi, F
   Sambruna, RM
   Reeves, JN
   Reynolds, CS
   Braito, V
AF Tombesi, F.
   Sambruna, R. M.
   Reeves, J. N.
   Reynolds, C. S.
   Braito, V.
TI X-ray evidence for the accretion disc-outflow connection in 3C 111
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; galaxies: active
ID ACTIVE GALACTIC NUCLEI; ULTRA-FAST OUTFLOWS; BLACK-HOLE;
   ABSORPTION-LINES; JET; WINDS; EMISSION; QUASAR; PHOTOIONIZATION;
   MECHANISM
AB We present the spectral analysis of three Suzaku X-ray Imaging Spectrometer observations of 3C 111 requested to monitor the predicted variability of its ultrafast outflow on similar to 7 d time-scales. We detect an ionized iron emission line in the first observation and a blueshifted absorption line in the second, when the flux is similar to 30 per cent higher. The location of the material is constrained at <0.006 pc from the variability. Detailed modelling supports an identification with ionized reflection off the accretion disc at similar to 20100rg from the black hole and a highly ionized and massive ultrafast outflow with velocity similar to 0.1c, respectively. The outflow is most probably accelerated by radiation pressure, but additional magnetic thrust cannot be excluded. The measured high outflow rate and mechanical energy support the claims that disc outflows may have a significant feedback role. This work provides the first direct evidence for an accretion discoutflow connection in a radio-loud active galactic nucleus, possibly linked also to the jet activity.
C1 [Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
   [Tombesi, F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
   [Tombesi, F.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Sambruna, R. M.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
   [Reeves, J. N.] Univ Keele, 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 XRAY, SUZAKU/A-1808-2009; 
OI Braito, Valentina/0000-0002-2629-4989
FU NASA [NNX10AR31G]
FX FT thanks A. P. Marscher for the useful discussion. CSR would like to
   thank NASA for support under Suzaku Guest Observer grant NNX10AR31G.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 418
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BP L89
EP L93
DI 10.1111/j.1745-3933.2011.01149.x
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SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700019
ER

PT J
AU Marley, MS
   Sengupta, S
AF Marley, Mark S.
   Sengupta, Sujan
TI Probing the physical properties of directly imaged gas giant exoplanets
   through polarization
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE polarization; scattering; planets and satellites: atmospheres; stars:
   atmospheres
ID DUST CLOUD FORMATION; ORBITING HR 8799; EDGE-ON DISK; EXTRASOLAR PLANET;
   BROWN DWARFS; T-DWARFS; SUBSTELLAR ATMOSPHERES; SURFACE GRAVITY; MU-M;
   YOUNG
AB It has been becoming clear that the atmospheres of the young, self-luminous extrasolar giant planets imaged to date are dusty. Planets with dusty atmospheres may exhibit detectable amounts of linear polarization in the near-infrared, as has been observed from some field L dwarfs. The asymmetry required in the thermal radiation field to produce polarization may arise either from the rotation-induced oblateness or from surface inhomogeneities, such as partial cloudiness. While it is not possible at present to predict the extent to which atmospheric dynamics on a given planet may produce surface inhomogeneities substantial enough to produce net non-zero disc-integrated polarization, the contribution of rotation-induced oblateness can be estimated. Using a self-consistent, spatially homogeneous atmospheric model and a multiple scattering polarization formalism for this class of exoplanets, we show that polarization of the order of 1 per cent may arise due to the rotation-induced oblateness of the planets. The degree of polarization for cloudy planets should peak at the same wavelengths at which the planets are brightest in the near-infrared. The observed polarization may be even higher if surface inhomogeneities exist and play a significant role. Polarized radiation from self-luminous gas giant exoplanets, if detected, provides an additional tool to characterize these young planets and a new method to constrain their surface gravity and masses.
C1 [Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Sengupta, Sujan] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
RP Marley, MS (reprint author), NASA, Ames Res Ctr, MS-245-3, Moffett Field, CA 94035 USA.
EM mark.s.marley@NASA.gov; sujan@iiap.res.in
OI Marley, Mark/0000-0002-5251-2943
FU NASA
FX We thank the anonymous referee for helpful comments that improved the
   manuscript. MSM recognizes the NASA Planetary Atmospheres Programme for
   support of this work.
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GA 848IA
UT WOS:000297043900032
ER

PT J
AU Kassin, SA
   Fogarty, L
   Goodsall, T
   Clarke, FJ
   Houghton, RWC
   Salter, G
   Thatte, N
   Tecza, M
   Davies, RL
   Weiner, BJ
   Willmer, CNA
   Salim, S
   Cooper, MC
   Newman, JA
   Bundy, K
   Conselice, CJ
   Koekemoer, AM
   Lin, LW
   Moustakas, LA
   Wang, T
AF Kassin, Susan A.
   Fogarty, L.
   Goodsall, T.
   Clarke, F. J.
   Houghton, R. W. C.
   Salter, G.
   Thatte, N.
   Tecza, M.
   Davies, Roger L.
   Weiner, Benjamin J.
   Willmer, C. N. A.
   Salim, Samir
   Cooper, Michael C.
   Newman, Jeffrey A.
   Bundy, Kevin
   Conselice, C. J.
   Koekemoer, A. M.
   Lin, Lihwai
   Moustakas, Leonidas A.
   Wang, Tao
TI Oxford SWIFT integral field spectrograph and multiwavelength
   observations of the Eagle galaxy at z=0.77
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: high-redshift; galaxies: interactions; galaxies: irregular;
   galaxies: kinematics and dynamics
ID STAR-FORMING GALAXIES; TULLY-FISHER RELATION; SIMILAR-TO 0.6; DATA
   REDUCTION SOFTWARE; INITIAL MASS FUNCTION; EXTENDED GROTH STRIP;
   TKRS/GOODS-N FIELD; FORMATION RATES; DYNAMICAL EVOLUTION; LUMINOSITY
   FUNCTION
AB The Eagle galaxy at a redshift of 0.77 is studied with the Oxford Short Wavelength Integral Field Spectrograph (SWIFT) and multiwavelength data from the All-wavelength Extended Groth strip International Survey (AEGIS). It was chosen from AEGIS because of the bright and extended emission in its slit spectrum. 3D kinematic maps of the Eagle reveal a gradient in velocity dispersion which spans 3575 +/- 10 km s-1 and a rotation velocity of 25 +/- 5 km s-1 uncorrected for inclination. Hubble Space Telescope images suggest it is close to face-on. In comparison with galaxies from AEGIS at similar redshifts, the Eagle is extremely bright and blue in the rest-frame optical, highly star forming, dominated by unobscured star formation and has a low metallicity for its size. This is consistent with its selection. The Eagle is likely undergoing a major merger and is caught in the early stage of a starburst when it has not yet experienced metal enrichment or formed the mass of dust typically found in star-forming galaxies.
C1 [Kassin, Susan A.; Fogarty, L.; Goodsall, T.; Clarke, F. J.; Houghton, R. W. C.; Salter, G.; Thatte, N.; Tecza, M.; Davies, Roger L.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
   [Fogarty, L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
   [Goodsall, T.; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Salter, G.] Univ New S Wales, Dept Astrophys, Sch Phys, Sydney, NSW 2052, Australia.
   [Weiner, Benjamin J.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Salim, Samir] Indiana Univ, Dept Astron, Bloomington, IN 47404 USA.
   [Cooper, Michael C.] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA USA.
   [Bundy, Kevin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94705 USA.
   [Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
   [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Lin, Lihwai] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
   [Wang, Tao] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kassin, SA (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
EM susan.kassin@nasa.gov
RI Salim, Siti Mawarni/B-7940-2010; Conselice, Christopher/B-4348-2013; 
OI Koekemoer, Anton/0000-0002-6610-2048; Salim, Siti
   Mawarni/0000-0001-5543-5384; Conselice, Christopher/0000-0003-1949-7638;
   Weiner, Benjamin/0000-0001-6065-7483; Moustakas,
   Leonidas/0000-0003-3030-2360
FU European Commission [MEXT-CT-2003-002792]; University of Oxford Physics
   Department; John Fell OUP Research Fund; Caltech Optical Observatories;
   Observational Astrophysics Rolling Grant at Oxford; Oxford Astrophysics
   PATT [ST/G004331/1]; NSF [AST00-71198, AST05-07483, AST08-08133];
   Balliol College, Oxford; STFC; NASA; NASA ATFP
FX The Oxford SWIFT integral field spectrograph is directly supported by a
   Marie Curie Excellence Grant from the European Commission
   (MEXT-CT-2003-002792, Team Leader: N. Thatte). It is also supported by
   additional funds from the University of Oxford Physics Department and
   the John Fell OUP Research Fund. Additional funds to host and support
   SWIFT were provided by Caltech Optical Observatories.; Additional
   support was provided for by the Observational Astrophysics Rolling Grant
   at Oxford and the Oxford Astrophysics PATT Linked Grant ST/G004331/1.
   The following NSF grants to the DEEP2 survey are acknowledged:
   AST00-71198, AST05-07483 and AST08-08133.; LF would like to acknowledge
   the generous support of the Foley-Bejar Scholarship through Balliol
   College, Oxford and the support of the STFC.; This work of LAM was
   carried out in part at Jet Propulsion Laboratory, California Institute
   of Technology, under a contract with NASA. LAM acknowledges support from
   the NASA ATFP programme.
NR 70
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 4
BP 2882
EP 2890
DI 10.1111/j.1365-2966.2011.19449.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IA
UT WOS:000297043900033
ER

PT J
AU Pint, CL
   Takei, K
   Kapadia, R
   Zheng, M
   Ford, AC
   Zhang, JJ
   Jamshidi, A
   Bardhan, R
   Urban, JJ
   Wu, M
   Ager, JW
   Oye, MM
   Javey, A
AF Pint, Cary L.
   Takei, Kuniharu
   Kapadia, Rehan
   Zheng, Maxwell
   Ford, Alexandra C.
   Zhang, Junjun
   Jamshidi, Arash
   Bardhan, Rizia
   Urban, Jeffrey J.
   Wu, Ming
   Ager, Joel W.
   Oye, Michael M.
   Javey, Ali
TI Rationally Designed, Three-Dimensional Carbon Nanotube Back-Contacts for
   Efficient Solar Devices
SO ADVANCED ENERGY MATERIALS
LA English
DT Article
DE carbon nanofibers; photoelectrochemistry; solar fuel; water splitting
ID HETEROJUNCTION ARRAYS; OPTICAL-ABSORPTION; WATER-PHOTOLYSIS; HYBRID
   MATERIALS; TIO2; ENERGY; CELLS; PHOTOELECTROCHEMISTRY; PHOTOCATALYSIS;
   ELECTRODES
C1 [Pint, Cary L.; Takei, Kuniharu; Kapadia, Rehan; Zheng, Maxwell; Ford, Alexandra C.; Zhang, Junjun; Jamshidi, Arash; Wu, Ming; Javey, Ali] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
   [Bardhan, Rizia; Urban, Jeffrey J.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Mat Sci, Mol Foundry, Berkeley, CA 94720 USA.
   [Oye, Michael M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Javey, A (reprint author), Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
EM ajavey@berkeley.edu
RI Pint, Cary/C-5053-2009; bardhan, rizia/A-9393-2010; Wu,
   Ming/J-9906-2012; Kapadia, Rehan/B-4100-2013; Pint, Cary/I-6785-2013;
   Bardhan, Rizia/B-4674-2014; Javey, Ali/B-4818-2013; 
OI Kapadia, Rehan/0000-0002-7611-0551; Ager, Joel/0000-0001-9334-9751
FU Berkeley Sensor and Actuator Center; Mohr Davidow Ventures; LDRD from
   Lawrence Berkeley National Laboratory (LBNL); Office of Science, Office
   of Basic Energy Sciences, Materials Sciences and Engineering Division,
   of the U. S. Department of Energy [DE-AC02-05CH11231]; Sloan Fellowship;
   World Class University, Sunchon National University
FX This work was partially funded by Berkeley Sensor and Actuator Center,
   and Mohr Davidow Ventures. The synthesis part of this work was supported
   by a LDRD from Lawrence Berkeley National Laboratory (LBNL). Reflectance
   measurements were performed using facilities in the Electronic Materials
   Program, LBNL, which is supported by supported by the Director, Office
   of Science, Office of Basic Energy Sciences, Materials Sciences and
   Engineering Division, of the U. S. Department of Energy under Contract
   No. DE-AC02-05CH11231. A.J. acknowledges a Sloan Fellowship and support
   from the World Class University program at Sunchon National University.
NR 34
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PU WILEY PERIODICALS, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA
SN 1614-6832
J9 ADV ENERGY MATER
JI Adv. Energy Mater.
PD NOV
PY 2011
VL 1
IS 6
BP 1040
EP 1045
DI 10.1002/aenm.201100436
PG 6
WC Chemistry, Physical; Energy & Fuels; Materials Science,
   Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Chemistry; Energy & Fuels; Materials Science; Physics
GA 848MU
UT WOS:000297056500010
ER

PT J
AU Russell, M
AF Russell, Michael
TI Professor Robert Shapiro (1935-2011) Tribute
SO ASTROBIOLOGY
LA English
DT Biographical-Item
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Russell, M (reprint author), CALTECH, Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 0
TC 0
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U1 0
U2 3
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 NOV
PY 2011
VL 11
IS 9
BP 837
EP 838
DI 10.1089/ast.2011.9280
PG 2
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
   Geology
GA 851JK
UT WOS:000297264300001
PM 22023384
ER

PT J
AU de Marcellus, P
   Bertrand, M
   Nuevo, M
   Westall, F
   d'Hendecourt, LL
AF de Marcellus, Pierre
   Bertrand, Marylene
   Nuevo, Michel
   Westall, Frances
   d'Hendecourt, Louis Le Sergeant
TI Prebiotic Significance of Extraterrestrial Ice Photochemistry: Detection
   of Hydantoin in Organic Residues
SO ASTROBIOLOGY
LA English
DT Article
DE Interstellar molecules; Ice; UV radiation; Organic matter; Prebiotic
   chemistry
ID INTERSTELLAR ICE; AMINO-ACIDS; MURCHISON METEORITE;
   ULTRAVIOLET-IRRADIATION; UV-IRRADIATION; DENSE CLOUDS; ANALOGS; ISO;
   PHOTOLYSIS; GAS
AB The delivery of extraterrestrial organic materials to primitive Earth from meteorites or micrometeorites has long been postulated to be one of the origins of the prebiotic molecules involved in the subsequent apparition of life. Here, we report on experiments in which vacuum UV photo-irradiation of interstellar/circumstellar ice analogues containing H2O, CH3OH, and NH3 led to the production of several molecules of prebiotic interest. These were recovered at room temperature in the semi-refractory, water-soluble residues after evaporation of the ice. In particular, we detected small quantities of hydantoin (2,4-imidazolidinedione), a species suspected to play an important role in the formation of poly- and oligopeptides. In addition, hydantoin is known to form under extraterrestrial, abiotic conditions, since it has been detected, along with various other derivatives, in the soluble part of organic matter of primitive carbonaceous meteorites. This result, together with other related experiments reported recently, points to the potential importance of the photochemistry of interstellar "dirty" ices in the formation of organics in Solar System materials. Such molecules could then have been delivered to the surface of primitive Earth, as well as other telluric (exo-) planets, to help trigger first prebiotic reactions with the capacity to lead to some form of primitive biomolecular activity.
C1 [de Marcellus, Pierre; d'Hendecourt, Louis Le Sergeant] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France.
   [Bertrand, Marylene; Westall, Frances] Univ Orleans, Ctr Biophys Mol, Orleans, France.
   [Nuevo, Michel] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
   [Nuevo, Michel] SETI Inst, Mountain View, CA USA.
   [d'Hendecourt, Louis Le Sergeant] CNRS, F-91405 Orsay, France.
RP d'Hendecourt, LL (reprint author), IAS CNRS Astrochim & Origines, Campus Orsay Bat 121, F-91400 Orsay, France.
EM ldh@ias.u-psud.fr
RI BERTRAND, Marylene/C-4892-2009
FU CNRS; PCMI; CNES "Exobiology Department"
FX We are indebted to Dr. G. Danger for enlightening discussions on the
   role of hydantoin in a prebiotic environment. This experiment was
   supported by the French program from CNRS, PCMI, and the CNES
   "Exobiology Department" (MICMOC Experiment). L.L.S.H. is grateful to Dr.
   Kensei Kobayashi for attracting our attention on the hydantoin molecule.
   Anonymous referees have been helpful to improve the quality of the
   manuscript.
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PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD NOV
PY 2011
VL 11
IS 9
BP 847
EP 854
DI 10.1089/ast.2011.0677
PG 8
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
   Geology
GA 851JK
UT WOS:000297264300003
PM 22059641
ER

PT J
AU Gowanlock, MG
   Patton, DR
   McConnell, SM
AF Gowanlock, M. G.
   Patton, D. R.
   McConnell, S. M.
TI A Model of Habitability Within the Milky Way Galaxy
SO ASTROBIOLOGY
LA English
DT Article
DE Astrobiology; Galactic evolution; Galactic habitable zone; Habitability;
   Supernovae
ID INITIAL MASS FUNCTION; STAR-FORMATION HISTORY; M-DWARF STARS; SOLAR
   NEIGHBORHOOD; IA SUPERNOVAE; COMPLEX LIFE; TERRESTRIAL PLANETS;
   DETERMINISTIC MODEL; LUMINOSITY FUNCTION; AGE DISTRIBUTION
AB We present a model of the galactic habitable zone (GHZ), described in terms of the spatial and temporal dimensions of the Galaxy that may favor the development of complex life. The Milky Way galaxy was modeled using a computational approach by populating stars and their planetary systems on an individual basis by employing Monte Carlo methods. We began with well-established properties of the disk of the Milky Way, such as the stellar number density distribution, the initial mass function, the star formation history, and the metallicity gradient as a function of radial position and time. We varied some of these properties and created four models to test the sensitivity of our assumptions. To assess habitability on the galactic scale, we modeled supernova rates, planet formation, and the time required for complex life to evolve. Our study has improved on other literature on the GHZ by populating stars on an individual basis and modeling Type II supernova (SNII) and Type Ia supernova (SNIa) sterilizations by selecting their progenitors from within this preexisting stellar population. Furthermore, we considered habitability on tidally locked and non-tidally locked planets separately and studied habitability as a function of height above and below the galactic midplane. In the model that most accurately reproduces the properties of the Galaxy, the results indicate that an individual SNIa is similar to 5.6x more lethal than an individual SNII on average. In addition, we predict that similar to 1.2% of all stars host a planet that may have been capable of supporting complex life at some point in the history of the Galaxy. Of those stars with a habitable planet, similar to 75% of planets are predicted to be in a tidally locked configuration with their host star. The majority of these planets that may support complex life are found toward the inner Galaxy, distributed within, and significantly above and below, the galactic midplane.
C1 [Gowanlock, M. G.] Univ Hawaii Manoa, Dept Informat & Comp Sci, Honolulu, HI 96822 USA.
   [Gowanlock, M. G.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
   [Gowanlock, M. G.; Patton, D. R.] Trent Univ, Dept Phys & Astron, Peterborough, ON K9J 7B8, Canada.
   [Gowanlock, M. G.; McConnell, S. M.] Trent Univ, Dept Comp & Informat Syst, Peterborough, ON K9J 7B8, Canada.
RP Gowanlock, MG (reprint author), Univ Hawaii, Dept Informat & Comp Sci, POST 310,1680 East West Rd, Honolulu, HI 96822 USA.
EM gowanloc@hawaii.edu
FU National Aeronautics and Space Administration through the NASA
   Astrobiology Institute [NNA08DA77A]; Natural Sciences and Engineering
   Research Council (NSERC) of Canada
FX This material is based upon work supported by the National Aeronautics
   and Space Administration through the NASA Astrobiology Institute under
   Cooperative Agreement No. NNA08DA77A issued through the Office of Space
   Science. D.R.P. gratefully acknowledges the financial support of a
   Discovery Grant from the Natural Sciences and Engineering Research
   Council (NSERC) of Canada. This paper also benefitted from the
   insightful comments of Jon Willis.
NR 66
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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 NOV
PY 2011
VL 11
IS 9
BP 855
EP 873
DI 10.1089/ast.2010.0555
PG 19
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
   Geology
GA 851JK
UT WOS:000297264300004
PM 22059554
ER

PT J
AU Livengood, TA
   Deming, LD
   A'Hearn, MF
   Charbonneau, D
   Hewagama, T
   Lisse, CM
   McFadden, LA
   Meadows, VS
   Robinson, TD
   Seager, S
   Wellnitz, DD
AF Livengood, Timothy A.
   Deming, L. Drake
   A'Hearn, Michael F.
   Charbonneau, David
   Hewagama, Tilak
   Lisse, Carey M.
   McFadden, Lucy A.
   Meadows, Victoria S.
   Robinson, Tyler D.
   Seager, Sara
   Wellnitz, Dennis D.
TI Properties of an Earth-Like Planet Orbiting a Sun-Like Star: Earth
   Observed by the EPOXI Mission
SO ASTROBIOLOGY
LA English
DT Article
DE Atmospheric composition; Biomarkers; Life detection; Habitability;
   Extrasolar terrestrial planets; EPOXI mission; Light curves; Exoplanets
ID EXTRASOLAR TERRESTRIAL PLANETS; DISK-AVERAGED SPECTRA; DEEP IMPACT;
   SYNTHETIC SPECTRA; LIGHT-CURVES; NUCLEUS; LIFE; PHOTOSYNTHESIS;
   DETECTABILITY; VARIABILITY
AB NASA's EPOXI mission observed the disc-integrated Earth and Moon to test techniques for reconnoitering extrasolar terrestrial planets, using the Deep Impact flyby spacecraft to observe Earth at the beginning and end of Northern Hemisphere spring, 2008, from a range of similar to 1/6 to 1/3 AU. These observations furnish high-precision and high-cadence empirical photometry and spectroscopy of Earth, suitable as "ground truth" for numerically simulating realistic observational scenarios for an Earth-like exoplanet with finite signal-to-noise ratio. Earth was observed at near-equatorial sub-spacecraft latitude on 18-19 March, 28-29 May, and 4-5 June (UT), in the range of 372-4540nm wavelength with low visible resolving power (lambda/Delta lambda=5-13) and moderate IR resolving power (lambda/Delta lambda=215-730). Spectrophotometry in seven filters yields light curves at similar to 372-948 nm filter-averaged wavelength, modulated by Earth's rotation with peak-to-peak amplitude of <= 20%. The spatially resolved Sun glint is a minor contributor to disc-integrated reflectance. Spectroscopy at 1100-4540 nm reveals gaseous water and carbon dioxide, with minor features of molecular oxygen, methane, and nitrous oxide. One-day changes in global cloud cover resulted in differences between the light curve beginning and end of <= 5%. The light curve of a lunar transit of Earth on 29 May is color-dependent due to the Moon's red spectrum partially occulting Earth's relatively blue spectrum. The "vegetation red edge" spectral contrast observed between two long-wavelength visible/near-IR bands is ambiguous, not clearly distinguishing between the verdant Earth diluted by cloud cover versus the desolate mineral regolith of the Moon. Spectrophotometry in at least one other comparison band at short wavelength is required to distinguish between Earth-like and Moon-like surfaces in reconnaissance observations. However, measurements at 850 nm alone, the high-reflectance side of the red edge, could be sufficient to establish periodicity in the light curve and deduce Earth's diurnal period and the existence of fixed surface units.
C1 [Livengood, Timothy A.; Deming, L. Drake; Hewagama, Tilak; McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Livengood, Timothy A.] Natl Ctr Earth & Space Sci Educ, Capital Hts, MD USA.
   [A'Hearn, Michael F.; Hewagama, Tilak; Wellnitz, Dennis D.] Univ Maryland, College Pk, MD 20742 USA.
   [Charbonneau, David] Harvard Univ, Cambridge, MA 02138 USA.
   [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
   [Meadows, Victoria S.; Robinson, Tyler D.] Univ Washington, Seattle, WA 98195 USA.
   [Seager, Sara] MIT, Cambridge, MA 02139 USA.
RP Livengood, TA (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
EM timothy.a.livengood@nasa.gov
RI Wellnitz, Dennis/B-4080-2012; Hewagama, T/C-8488-2012; Livengood,
   Timothy/C-8512-2012; McFadden, Lucy-Ann/I-4902-2013; Lisse,
   Carey/B-7772-2016; 
OI McFadden, Lucy-Ann/0000-0002-0537-9975; Lisse,
   Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X
FU NASA; EPOXI mission
FX This work was supported by the NASA Discovery Program and the EPOXI
   mission. The authors gratefully acknowledge the contributions of the
   Deep Impact/EPOXI operations team at the Jet Propulsion Laboratory,
   without whom the unique observations described here could not have been
   accomplished, and the paleobotanical assistance of A.C. Dooley of the
   Virginia Museum of Natural History.
NR 48
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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 NOV
PY 2011
VL 11
IS 9
BP 907
EP 930
DI 10.1089/ast.2011.0614
PG 24
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
   Geology
GA 851JK
UT WOS:000297264300008
PM 22077375
ER

PT J
AU Sunderland-Groves, JL
   Slayback, DA
   Balinga, MPB
   Sunderland, TCH
AF Sunderland-Groves, J. L.
   Slayback, D. A.
   Balinga, M. P. Bessike
   Sunderland, T. C. H.
TI Impacts of co-management on western chimpanzee (Pan troglodytes verus)
   habitat and conservation in Nialama Classified Forest, Republic of
   Guinea: a satellite perspective
SO BIODIVERSITY AND CONSERVATION
LA English
DT Article
DE Chimpanzees; Classified forest; Natural resource management;
   Co-management; Guinea
ID BIODIVERSITY CONSERVATION; PROTECTED AREA; PRIMATES; DECLINE; AFRICA
AB The first model for co-management between local communities and government towards the sustainable utilization of forested regions in Republic of Guinea was established in the Nialama Classified Forest in 1999. Technical and financial support was provided by USAID to develop local natural resource management capacity. Long-term local chimpanzee monitoring provided the basis for delimiting the boundaries of core areas for strict protection which continue to provide refuge to the resident chimpanzee population. Using satellite imagery, we reviewed the impacts of co-management on key chimpanzee habitat between 1986 and 2009. Degradation statistics show that land cover change within areas delimited as critical chimpanzee habitat inside of the Classified Forest was far less compared to the Classified Forest as a whole, or within a 5 km buffer zone. Comparatively, critical chimpanzee habitat located outside of the Nialama Classified Forest suffered the most degradation. Here we discuss the impacts of co-management on chimpanzee habitat and causal factors surrounding the continued survival of chimpanzees in Nialama.
C1 [Sunderland-Groves, J. L.; Balinga, M. P. Bessike; Sunderland, T. C. H.] Ctr Int Forestry Res, Bogor 16000, Indonesia.
   [Slayback, D. A.] Sci Syst & Applicat Inc, NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Sunderland-Groves, JL (reprint author), Ctr Int Forestry Res, POB 0113 BOCBD, Bogor 16000, Indonesia.
EM takamanda@aol.com
FU United States Agency for International Development (USAID); Center for
   International Forestry Research (CIFOR)
FX We would like to thank the Ministry of Forestry of Guinea for their
   permission to carry out this study with particular thanks to M. Oulare
   Aboubakar. We thank the United States Agency for International
   Development (USAID) for providing funding to the LAMIL project and to
   the Center for International Forestry Research (CIFOR) for supporting
   this study. Gray Tappan of USGS provided useful comments on the remote
   sensing of landcover in this region. Many individuals have worked
   tirelessly in the region for a number of years and we particularly thank
   Janis Carter responsible for the design and supervision of the
   chimpanzee field data reported upon here.
NR 34
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0960-3115
J9 BIODIVERS CONSERV
JI Biodivers. Conserv.
PD NOV
PY 2011
VL 20
IS 12
BP 2745
EP 2757
DI 10.1007/s10531-011-0102-4
PG 13
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 850MX
UT WOS:000297200000012
ER

PT J
AU Rodriguez, S
   Le Mouelic, S
   Rannou, P
   Sotin, C
   Brown, RH
   Barnes, JW
   Griffith, CA
   Burgalat, J
   Baines, KH
   Buratti, BJ
   Clark, RN
   Nicholson, PD
AF Rodriguez, S.
   Le Mouelic, S.
   Rannou, P.
   Sotin, C.
   Brown, R. H.
   Barnes, J. W.
   Griffith, C. A.
   Burgalat, J.
   Baines, K. H.
   Buratti, B. J.
   Clark, R. N.
   Nicholson, P. D.
TI Titan's cloud seasonal activity from winter to spring with Cassini/VIMS
SO ICARUS
LA English
DT Article
DE Satellites, Atmospheres; Titan; Meteorology
ID HUYGENS LANDING SITE; KECK ADAPTIVE OPTICS; SATURNS MOON TITAN;
   TROPOSPHERIC CLOUDS; MIDLATITUDE CLOUDS; METHANE CYCLE; SOUTH-POLE;
   SURFACE; ATMOSPHERE; WINDS
AB Since Saturn orbital insertion in July 2004, the Cassini orbiter has been observing Titan throughout most of the northern winter season (October 2002 August 2009) and the beginning of spring, allowing a detailed monitoring of Titan's cloud coverage at high spatial resolution with close flybys on a monthly basis. This study reports on the analysis of all the near-infrared images of Titan's clouds acquired by the Visual and Infrared Mapping Spectrometer (VIMS) during 67 targeted flybys of Titan between July 2004 and April 2010.
   The VIMS observations show numerous sporadic clouds at southern high and mid-latitudes, rare clouds in the equatorial region, and reveal a long-lived cloud cap above the north pole, ubiquitous poleward of 60 degrees N. These observations allow us to follow the evolution of the cloud coverage during almost a 6-year period including the equinox, and greatly help to further constrain global circulation models (GCMs). After 4 years of regular outbursts observed by Cassini between 2004 and 2008, southern polar cloud activity started declining, and completely ceased 1 year before spring equinox. The extensive cloud system over the north pole, stable between 2004 and 2008, progressively fractionated and vanished as Titan entered into northern spring. At southern mid-latitudes, clouds were continuously observed throughout the VIMS observing period, even after equinox, in a latitude band between 30 S and 60 S. During the whole period of observation, only a dozen clouds were observed closer to the equator, though they were slightly more frequent as equinox approached.
   We also investigated the distribution of clouds with longitude. We found that southern polar clouds, before disappearing in mid-2008, were systematically concentrated in the leading hemisphere of Titan, in particular above and to the east of Ontario Lacus, the largest reservoir of hydrocarbons in the area. Clouds are also non-homogeneously distributed with longitude at southern mid-latitudes. The n = 2-mode wave pattern of the distribution, observed since 2003 by Earth-based telescopes and confirmed by our Cassini observations, may be attributed to Saturn's tides.
   Although the latitudinal distribution of clouds is now relatively well reproduced and understood by the GCMs, the non-homogeneous longitudinal distributions and the evolution of the cloud coverage with seasons still need investigation. If the observation of a few single clouds at the tropics and at northern mid-latitudes late in winter and at the start of spring cannot be further interpreted for the moment, the obvious shutdown of the cloud activity at Titan's poles provides clear signs of the onset of the general circulation turnover that is expected to accompany the beginning of Titan's northern spring. According to our GCM, the persistence of clouds at certain latitudes rather suggests a 'sudden' shift in near future of the meteorology into the more illuminated hemisphere. Finally, the observed seasonal change in cloud activity occurred with a significant time lag that is not predicted by our model. This may be due to an overall methane humidity at Titan's surface higher than previously expected. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Rodriguez, S.] Univ Paris 07, Lab AIM, CNRS CEA Saclay, DSM IRFU SAp,Ctr Orme Merisiers, F-91191 Gif Sur Yvette, France.
   [Le Mouelic, S.; Sotin, C.] Univ Nantes, Lab Planetol & Geodynam, UMR CNRS 6112, F-44322 Nantes 3, France.
   [Rannou, P.; Burgalat, J.] Univ Reims, Grp Spect Mol & Atmospher, UFR Sci Exactes & Nat, UMR CNRS 6089, F-51687 Reims 2, France.
   [Sotin, C.; Buratti, B. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Brown, R. H.; Griffith, C. A.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
   [Brown, R. H.; Griffith, C. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
   [Baines, K. H.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
   [Clark, R. N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
   [Nicholson, P. D.] Cornell Univ, Ithaca, NY 14853 USA.
RP Rodriguez, S (reprint author), Univ Paris 07, Lab AIM, CNRS CEA Saclay, DSM IRFU SAp,Ctr Orme Merisiers, Bat 709, F-91191 Gif Sur Yvette, France.
EM sebastien.rodriguez@cea.fr
RI Barnes, Jason/B-1284-2009; RANNOU, Pascal/I-9059-2012; Rodriguez,
   Sebastien/H-5902-2016
OI Barnes, Jason/0000-0002-7755-3530; Rodriguez,
   Sebastien/0000-0003-1219-0641
FU Centre National de la Recherche Scientifique, Institut National des
   Sciences de l'Univers; French Centre National d'Etudes Spatiales (CNES);
   ANR
FX This work benefited from financial support from the Centre National de
   la Recherche Scientifique, Institut National des Sciences de l'Univers,
   from the French Centre National d'Etudes Spatiales (CNES) and from the
   ANR (project Exoclimat). Part of this work was performed at the Jet
   Propulsion Laboratory, California Institute of Technology, under
   contract to the National Aeronautics and Space Administration. We
   gratefully acknowledge the long years of work done by the entire Cassini
   and VIMS teams that allowed (and still allow) the acquisition of these
   outstanding sets of data. We also thank the two anonymous reviewers for
   very insightful comments and suggestions that helped the manuscript.
NR 76
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SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 89
EP 110
DI 10.1016/j.icarus.2011.07.031
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100009
ER

PT J
AU Barnes, JW
   Bow, J
   Schwartz, J
   Brown, RH
   Soderblom, JM
   Hayes, AG
   Vixie, G
   Le Mouelic, S
   Rodriguez, S
   Sotin, C
   Jaumann, R
   Stephan, K
   Soderblom, LA
   Clark, RN
   Buratti, BJ
   Baines, KH
   Nicholson, PD
AF Barnes, Jason W.
   Bow, Jacob
   Schwartz, Jacob
   Brown, Robert H.
   Soderblom, Jason M.
   Hayes, Alexander G.
   Vixie, Graham
   Le Mouelic, Stephane
   Rodriguez, Sebastien
   Sotin, Christophe
   Jaumann, Ralf
   Stephan, Katrin
   Soderblom, Laurence A.
   Clark, Roger N.
   Buratti, Bonnie J.
   Baines, Kevin H.
   Nicholson, Philip D.
TI Organic sedimentary deposits in Titan's dry lakebeds: Probable evaporite
SO ICARUS
LA English
DT Article
DE Titan
ID SURFACE; LAKES; CASSINI/VIMS; DIVERSITY; HAZE; MARS
AB We report the discovery of organic sedimentary deposits at the bottom of dry lakebeds near Titan's north pole in observations from the Cassini Visual and Infrared Mapping Spectrometer (VIMS). We show evidence that the deposits are evaporitic, making Titan just the third known planetary body with evaporitic processes after Earth and Mars, and is the first that uses a solvent other than water. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Barnes, Jason W.; Bow, Jacob; Schwartz, Jacob; Vixie, Graham] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
   [Schwartz, Jacob] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
   [Brown, Robert H.; Soderblom, Jason M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
   [Soderblom, Jason M.; Nicholson, Philip D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Hayes, Alexander G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Le Mouelic, Stephane] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR6112, F-44035 Nantes, France.
   [Rodriguez, Sebastien] Ctr Orme Merisiers, DAPNIA Sap, Ctr Tude Saclay E, Lab AIM, F-91191 Gif Sur Yvette, France.
   [Sotin, Christophe; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Jaumann, Ralf; Stephan, Katrin] Inst Planetary Res, DLR, D-12489 Berlin, Germany.
   [Soderblom, Laurence A.] US Geol Survey, Astrogeol Div, Flagstaff, AZ 86001 USA.
   [Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA.
   [Baines, Kevin H.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
RP Barnes, JW (reprint author), Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
EM jwbarnes@uidaho.edu
RI Barnes, Jason/B-1284-2009; Hayes, Alexander/P-2024-2014; Schwartz,
   Jacob/L-5744-2015; Rodriguez, Sebastien/H-5902-2016; 
OI Barnes, Jason/0000-0002-7755-3530; Hayes, Alexander/0000-0001-6397-2630;
   Schwartz, Jacob/0000-0001-9636-8181; Rodriguez,
   Sebastien/0000-0003-1219-0641; Soderblom, Jason/0000-0003-3715-6407
FU Cassini Project
FX The authors acknowledge support from the Cassini Project and helpful
   discussions with Ralph D. Lorenz and Christopher P. McKay.
NR 35
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SN 0019-1035
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JI Icarus
PD NOV
PY 2011
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IS 1
BP 136
EP 140
DI 10.1016/j.icarus.2011.08.022
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100013
ER

PT J
AU Irwin, PGJ
   Teanby, NA
   Davis, GR
   Fletcher, LN
   Orton, GS
   Tice, D
   Hurley, J
   Calcutt, SB
AF Irwin, P. G. J.
   Teanby, N. A.
   Davis, G. R.
   Fletcher, L. N.
   Orton, G. S.
   Tice, D.
   Hurley, J.
   Calcutt, S. B.
TI Multispectral imaging observations of Neptune's cloud structure with
   Gemini-North
SO ICARUS
LA English
DT Article
DE Neptune, Atmosphere; Radiative transfer; Atmospheres, Composition
ID INFRARED-ABSORPTION SPECTRA; MU-M; ATMOSPHERIC CIRCULATION;
   RADIATIVE-TRANSFER; OPTICAL-CONSTANTS; METHANE ABUNDANCE; SOLID METHANE;
   OUTER PLANETS; URANUS; TEMPERATURES
AB Observations of Neptune were made in September 2009 with the Gemini-North Telescope in Hawaii, using the NIFS instrument in the H-band covering the wavelength range 1.477-1.803 mu m. Observations were acquired in adaptive optics mode and have a spatial resolution of approximately 0.15-0.25".
   The observations were analysed with a multiple-scattering retrieval algorithm to determine the opacity of clouds at different levels in Neptune's atmosphere. We find that the observed spectra at all locations are very well fit with a model that has two thin cloud layers, one at a pressure level of similar to 2 bar all over the planet and an upper cloud whose pressure level varies from 0.02 to 0.08 bar in the bright mid-latitude region at 20-40 degrees S to as deep as 0.2 bar near the equator. The opacity of the upper cloud is found to vary greatly with position, but the opacity of the lower cloud deck appears remarkably uniform, except for localised bright spots near 60 degrees S and a possible slight clearing near the equator.
   A limb-darkening analysis of the observations suggests that the single-scattering albedo of the upper cloud particles varies from similar to 0.4 in regions of low overall albedo to close to 1.0 in bright regions, while the lower cloud is consistent with particles that have a single-scattering albedo of similar to 0.75 at this wavelength, similar to the value determined for the main cloud deck in Uranus' atmosphere. The Henyey-Greenstein scattering particle asymmetry of particles in the upper cloud deck are found to be in the range g similar to 0.6-0.7 (i.e. reasonably strongly forward scattering).
   Numerous bright clouds are seen near Neptune's south pole at a range of pressure levels and at latitudes between 60 and 70 degrees S. Discrete clouds were seen at the pressure level of the main cloud deck (similar to 2 bar) at 60 degrees S on three of the six nights observed. Assuming they are the same feature we estimate the rotation rate at this latitude and pressure to be 13.2 +/- 0.1 h. However, the observations are not entirely consistent with a single non-evolving cloud feature, which suggests that the cloud opacity or albedo may vary very rapidly at this level at a rate not seen in any other giant-planet atmosphere. (C) 2011 Elsevier Inc. All rights reserved,
C1 [Irwin, P. G. J.; Fletcher, L. N.; Tice, D.; Hurley, J.; Calcutt, S. B.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
   [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England.
   [Davis, G. R.] Joint Astron Ctr, Hilo, HI 96720 USA.
   [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Irwin, PGJ (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
EM irwin@atm.ox.ac.uk
RI Fletcher, Leigh/D-6093-2011; 
OI Fletcher, Leigh/0000-0001-5834-9588; Calcutt, Simon/0000-0002-0102-3170;
   Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X
FU United Kingdom Science and Technology Facilities Council; NASA
FX We are grateful to the United Kingdom Science and Technology Facilities
   Council for funding this research, our support astronomers: Richard
   McDermid and Chad Trujillo, and also to Ilona Soechting in the UK Gemini
   Office. Glenn Orton was supported by a Grant from NASA to the Jet
   Propulsion Laboratory, California Institute of Technology. The Gemini
   Observatory is operated by the Association of Universities for Research
   in Astronomy, Inc., under a cooperative agreement with the NSF on behalf
   of the Gemini partnership: the National Science Foundation (United
   States), the Science and Technology Facilities Council (United Kingdom),
   the National Research Council (Canada), CONICYT (Chile), the Australian
   Research Council (Australia), Ministerio da Ciencia e Tecnologia
   (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva
   (Argentina).
NR 61
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SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 141
EP 158
DI 10.1016/j.icarus.2011.08.005
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100014
ER

PT J
AU Farrell, WM
   Halekas, JS
   Stubbs, TJ
   Delory, GT
   Killen, RM
   Hartle, RE
   Collier, MR
AF Farrell, W. M.
   Halekas, J. S.
   Stubbs, T. J.
   Delory, G. T.
   Killen, R. M.
   Hartle, R. E.
   Collier, M. R.
TI Regarding the possible generation of a lunar nightside exo-ionosphere
SO ICARUS
LA English
DT Article
DE Moon; Ionospheres
ID PLASMA WAKE; EXPANSION; HYDROGEN; HELIUM; VACUUM; FIELDS; DUST
AB The non-condensing neutral helium exosphere is at its most concentrated levels on the cold lunar nightside. We show herein that these He atoms are susceptible to impact ionization from primary and secondary electrons flowing in the vicinity of the negatively-charged nightside lunar surface. The secondary electron beams are a relatively recent discovery and are found to be emitted from the nightside surface at energies consistent with the negative surface potential. The effect is to create an electron impact-created ionosphere in nightside regions, possibly especially potent within polar craters. Published by Elsevier Inc.
C1 [Farrell, W. M.; Stubbs, T. J.; Killen, R. M.; Hartle, R. E.; Collier, M. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Halekas, J. S.; Delory, G. T.; Hartle, R. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Stubbs, T. J.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
   [Farrell, W. M.; Halekas, J. S.; Stubbs, T. J.; Delory, G. T.; Killen, R. M.; Collier, M. R.] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA.
EM william.m.farrell@nasa.gov
RI Killen, Rosemary/E-7127-2012; Collier, Michael/I-4864-2013; Stubbs,
   Timothy/I-5139-2013; Farrell, William/I-4865-2013; 
OI Collier, Michael/0000-0001-9658-6605; Stubbs,
   Timothy/0000-0002-5524-645X; Halekas, Jasper/0000-0001-5258-6128
NR 24
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SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 169
EP 172
DI 10.1016/j.icarus.2011.08.013
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100016
ER

PT J
AU Howett, CJA
   Spencer, JR
   Schenk, P
   Johnson, RE
   Paranicas, C
   Hurford, TA
   Verbiscer, A
   Segura, M
AF Howett, C. J. A.
   Spencer, J. R.
   Schenk, P.
   Johnson, R. E.
   Paranicas, C.
   Hurford, T. A.
   Verbiscer, A.
   Segura, M.
TI A high-amplitude thermal inertia anomaly of probable magnetospheric
   origin on Saturn's moon Mimas
SO ICARUS
LA English
DT Article
DE Satellites, Surfaces; Satellites, Composition; Magnetospheres
ID EUROPA; TEMPERATURES
AB Spectral maps of Mimas' daytime thermal emission show a previously unobserved thermal anomaly on Mimas' surface. A sharp V-shaped boundary, centered at 0 degrees N and 180 W, separates relatively warm daytime temperatures from a cooler anomalous region occupying low- to mid-latitudes on the leading hemisphere. Subsequent observations show the anomalous region is also warmer than its surroundings at night, indicating high thermal inertia. Thermal inertia in the anomalous region is 66 +/- 23 J m(-2) K(-1) s(1/2), compared to <16 J m(-2) K(-1) s(1/2) outside the anomaly. Bolometric Bond albedos are similar between the two regions, in the range 0.49-0.70. The mapped portion of the thermally anomalous region coincides in shape and location to a region of high-energy electron deposition from Saturn's magnetosphere, which also has unusually high near-UV reflectance. It is therefore likely that high-energy electrons, which penetrate Mimas' surface to the centimeter depths probed by diurnal temperature variations, also alter the surface texture, dramatically increasing its thermal inertia. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Howett, C. J. A.; Spencer, J. R.] SW Res Inst, Boulder, CO 80304 USA.
   [Schenk, P.] Lunar & Planetary Inst, Houston, TX USA.
   [Johnson, R. E.; Verbiscer, A.] Univ Virginia, Charlottesville, VA 22904 USA.
   [Paranicas, C.] Johns Hopkins Univ, Laurel, MD 20723 USA.
   [Hurford, T. A.; Segura, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Howett, CJA (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80304 USA.
EM howett@boulder.swri.edu
RI Hurford, Terry/F-2625-2012; Paranicas, Christopher/B-1470-2016
OI Paranicas, Christopher/0000-0002-4391-8255
FU Cassini project
FX The authors would like to thank the Cassini project and especially the
   CIRS team that made these data possible. They would also like to thank
   Elias Roussos for his work in updating the energy deposition contours
   and for help interpreting the Cassini/MIMI data at the highest energies.
   This work was supported by the Cassini project.
NR 24
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 221
EP 226
DI 10.1016/j.icarus.2011.09.007
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100021
ER

PT J
AU Villanueva, GL
   Mumma, MJ
   DiSanti, MA
   Bonev, BP
   Gibb, EL
   Magee-Sauer, K
   Blake, GA
   Salyk, C
AF Villanueva, G. L.
   Mumma, M. J.
   DiSanti, M. A.
   Bonev, B. P.
   Gibb, E. L.
   Magee-Sauer, K.
   Blake, G. A.
   Salyk, C.
TI The molecular composition of Comet C/2007 W1 (Boattini): Evidence of a
   peculiar outgassing and a rich chemistry
SO ICARUS
LA English
DT Article
DE Comets, Composition; Infrared observations; Astrobiology; Cosmochemistry
ID O1 HALE-BOPP; C/1996 B2 HYAKUTAKE; ORTHO-PARA RATIO; PARENT VOLATILES;
   CARBON-MONOXIDE; SPECTROSCOPIC DATABASE; ROTATIONAL TEMPERATURES;
   ORGANIC COMPOSITION; SPIN TEMPERATURES; Q2 MACHHOLZ
AB We measured the chemical composition of Comet C/2007 W1 (Boattini) using the long-slit echelle grating spectrograph at Keck-2 (NIRSPEC) on 2008 July 9 and 10. We sampled 11 volatile species (H2O, OH*, C2H6, CH3OH, H2CO, CH4, HCN, C2H2, NH3, NH2, and CO), and retrieved three important cosmogonic indicators: the ortho-para ratios of H2O and CH4, and an upper-limit for the D/H ratio in water. The abundance ratios of almost all trace volatiles (relative to water) are among the highest ever observed in a comet. The comet also revealed a complex outgassing pattern, with some volatiles (the polar species H2O and CH3OH) presenting very asymmetric spatial profiles (extended in the anti-sunward hemisphere), while others (e.g., C2H6 and HCN) showed particularly symmetric profiles. We present emission profiles measured along the Sun-comet line for all observed volatiles, and discuss different production scenarios needed to explain them. We interpret the emission profiles in terms of release from two distinct moieties of ice, the first being clumps of mixed ice and dust released from the nucleus into the sunward hemisphere. The second moiety considered is very small grains of nearly pure polar ice (water and methanol, without dark material or apolar volatiles). Such grains would sublimate only very slowly, and could be swept into the anti-sunward hemisphere by radiation pressure and solar-actuated non-gravitational jet forces, thus providing an extended source in the anti-sunward hemisphere. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Villanueva, G. L.; Mumma, M. J.; DiSanti, M. A.; Bonev, B. P.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Villanueva, G. L.; Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Gibb, E. L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA.
   [Magee-Sauer, K.] Rowan Univ, Dept Phys & Astron, Glassboro, NJ 08028 USA.
   [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Salyk, C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Villanueva, GL (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Mailstop 690-3, Greenbelt, MD 20771 USA.
EM Geronimo.Villanueva@nasa.gov
RI mumma, michael/I-2764-2013; Magee-Sauer, Karen/K-6061-2015
OI Magee-Sauer, Karen/0000-0002-4979-9875
FU NASA's Astrobiology Institute [RTOP 344-53-51]; NASA [RTOPs 344-32-07,
   08-PAST08-0034, 08-PATM08-0031]; NSF [AST-0807939]; NSF RUI; W.M. Keck
   Foundation
FX G.L.V., M.J.M., M.A.D. and B.P.B. acknowledge support from NASA's
   Astrobiology Institute (RTOP 344-53-51), and NASA's Planetary
   Atmospheres and Astronomy Programs (RTOPs 344-32-07, 08-PAST08-0034,
   08-PATM08-0031). B.P.B. and E.L.G. acknowledge support from the NSF
   Astronomy and Astrophysics Research Grants Program (AST-0807939), and
   KMS from the NSF RUI Program. GAB acknowledges support from the NASA
   Origins of Solar Systems program. We thank James Lyke and the staff of
   Keck Observatory for general support. The data presented herein were
   obtained at the W.M. Keck Observatory operated as a scientific
   partnership among CalTech, UCLA, and NASA. This Observatory was made
   possible by the generous financial support of the W.M. Keck Foundation.
   The authors wish to recognize and acknowledge the very significant
   cultural role and reverence that the summit of Mauna Kea has always had
   within the indigenous Hawaiian community. We are most fortunate to have
   the opportunity to conduct observations from this mountain.
NR 57
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U2 6
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 227
EP 240
DI 10.1016/j.icarus.2011.08.024
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100022
ER

PT J
AU Brozovic, M
   Benner, LAM
   Taylor, PA
   Nolan, MC
   Howell, ES
   Magri, C
   Scheeres, DJ
   Giorgini, JD
   Pollock, JT
   Pravec, P
   Galad, A
   Fang, J
   Margot, JL
   Busch, MW
   Shepard, MK
   Reichart, DE
   Ivarsen, KM
   Haislip, JB
   LaCluyze, AP
   Jao, J
   Slade, MA
   Lawrence, KJ
   Hicks, MD
AF Brozovic, Marina
   Benner, Lance A. M.
   Taylor, Patrick A.
   Nolan, Michael C.
   Howell, Ellen S.
   Magri, Christopher
   Scheeres, Daniel J.
   Giorgini, Jon D.
   Pollock, Joseph T.
   Pravec, Petr
   Galad, Adrian
   Fang, Julia
   Margot, Jean-Luc
   Busch, Michael W.
   Shepard, Michael K.
   Reichart, Daniel E.
   Ivarsen, Kevin M.
   Haislip, Joshua B.
   LaCluyze, Aaron P.
   Jao, Joseph
   Slade, Martin A.
   Lawrence, Kenneth J.
   Hicks, Michael D.
TI Radar and optical observations and physical modeling of triple
   near-Earth Asteroid (136617) 1994 CC
SO ICARUS
LA English
DT Article
DE Asteroids; Near-Earth objects; Radar observations; Satellites of
   asteroids
ID SMALL BINARY ASTEROIDS; OBJECT POPULATION; TIDAL EVOLUTION; DYNAMICS;
   SYSTEMS; ORIGIN; KW4
AB We report radar, photometric, and spectroscopic observations of near-Earth Asteroid (136617) 1994 CC. The radar measurements were obtained at Goldstone (8560 MHz, 3.5 cm) and Arecibo (2380 MHz, 12.6 cm) on 9 days following the asteroid's approach within 0.0168 AU on June 10, 2009. 1994 CC was also observed with the Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT) on May 21 and June 1-3. Visible-wavelength spectroscopy was obtained with the 5-m Hale telescope at Palomar on August 25. Delay-Doppler radar images reveal that 1994 CC is a triple system; along with (153591) 2001 SN263, this is only the second confirmed triple in the near-Earth population. Photometry obtained with PROMPT yields a rotation period for the primary P = 2.38860 +/- 0.00009 h and a lightcurve amplitude of similar to 0.1 mag suggesting a shape with low elongation. Hale telescope spectroscopy indicates that 1994 CC is an Sq-class object. Delay-Doppler radar images and shape modeling reveal that the primary has an effective diameter of 0.62 +/- 0.06 km, low pole-on elongation, few obvious surface features, and a prominent equatorial ridge and sloped hemispheres that closely resemble those seen on the primary of binary near-Earth Asteroid (66391) 1999 KW4. Detailed orbit fitting reported separately by Fang et al. (Fang, J., Margot, J.-L., Brozovic, M., Nolan, MC., Benner, LAM., Taylor, P.A. [2011]. Astron. J. 141, 154-168) gives a mass of the primary of 2.6 x 10(11) kg that, coupled with the effective diameter, yields a bulk density of 2.1 +/- 0.6 g cm(-3). The images constrain the diameters of the inner and outer satellites to be 113 +/- 30 m and 80 +/- 30 m, respectively. The inner satellite has a semimajor axis of similar to 1.7 km (similar to 5.5 primary radii), an orbital period of similar to 30 h, and its Doppler dispersion suggests relatively slow rotation, 26 +/- 12 h, consistent with spin-orbit lock. The outer satellite has an orbital period of similar to 9 days and a rotation period of 14 +/- 7 h, establishing that the rotation is not spin-orbit locked. Among all binary and triple systems observed by radar, at least 25% (7/28) have a satellite that rotates more rapidly than its orbital period. This suggests that asynchronous configurations with P(rotation) < P(orbital) are relatively common among multiple systems in the near-Earth population. 1994 CC's outer satellite has an observed maximum separation from the primary of similar to 5.7 km (similar to 18.4 primary radii) that is the largest separation relative to primary radius seen to date among all 36 known binary and triple NEA systems. 1994 CC, (153591) 2001 SN263, and 1998 ST27 are the only triple and binary systems known with satellite separations >10 primary radii, suggesting either a detection bias, or that such widely-separated satellites are relatively uncommon in NEA multiple systems. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Brozovic, Marina; Benner, Lance A. M.; Giorgini, Jon D.; Jao, Joseph; Slade, Martin A.; Lawrence, Kenneth J.; Hicks, Michael D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Taylor, Patrick A.; Nolan, Michael C.; Howell, Ellen S.] Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA.
   [Magri, Christopher] Univ Maine, Farmington, ME 04938 USA.
   [Scheeres, Daniel J.] Univ Colorado, Boulder, CO 80309 USA.
   [Pollock, Joseph T.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28607 USA.
   [Pravec, Petr; Galad, Adrian] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic.
   [Galad, Adrian] FMFI UK, Dept Astronomy Phys Earth & Meteorol, Modra Observ, SK-84248 Bratislava, Slovakia.
   [Fang, Julia; Margot, Jean-Luc] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [Margot, Jean-Luc; Busch, Michael W.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
   [Shepard, Michael K.] Bloomsburg Univ, Dept Geog & Geosci, Bloomsburg, PA 17815 USA.
   [Reichart, Daniel E.; Ivarsen, Kevin M.; Haislip, Joshua B.; LaCluyze, Aaron P.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
RP Brozovic, M (reprint author), CALTECH, Jet Prop Lab, Mail Stop 301-121, Pasadena, CA 91109 USA.
EM Marina.Brozovic@jpl.nasa.gov
RI Margot, Jean-Luc/A-6154-2012; Nolan, Michael/H-4980-2012; Pravec,
   Petr/G-9037-2014; Galad, Adrian/G-9011-2014
OI Margot, Jean-Luc/0000-0001-9798-1797; Nolan,
   Michael/0000-0001-8316-0680; 
FU Grant Agency of the Czech Republic [205/09/1107]; Slovak Grant Agency
   for Science VEGA [2/0016/09]; NASA
FX We thank Kevin Walsh and Darin Ragozzine for their insightful reviews,
   which improved our manuscript. We thank the Arecibo and Goldstone
   technical and support staffs for help with the radar observations. The
   Arecibo Observatory is part of the National Astronomy and Ionosphere
   Center (NAIC), which is operated by Cornell University under a
   cooperative agreement with the National Science Foundation (NSF). The
   work at Ondrejov has been supported by the Grant Agency of the Czech
   Republic, Grant 205/09/1107. The work at Modra has been supported by the
   Slovak Grant Agency for Science VEGA, Grant 2/0016/09. Some of this work
   was performed at the Jet Propulsion Laboratory, California Institute of
   Technology, under contract with National Aeronautics and Space
   Administration (NASA). This material is based in part upon work
   supported by NASA under the Science Mission Directorate Research and
   Analysis Programs.
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SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 241
EP 256
DI 10.1016/j.icarus.2011.09.002
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100023
ER

PT J
AU Baillie, K
   Colwell, JE
   Lissauer, JJ
   Esposito, LW
   Sremcevic, M
AF Baillie, Kevin
   Colwell, Joshua E.
   Lissauer, Jack J.
   Esposito, Larry W.
   Sremcevic, Miodrag
TI Waves in Cassini UVIS stellar occultations 2. The C ring
SO ICARUS
LA English
DT Article
DE Saturn, Rings
ID SATURNS RINGS; DENSITY WAVES; RESONANCE STRUCTURES; RADIO OCCULTATION;
   B-RING; DIVISION; SYSTEM
AB We performed a complete wavelet analysis of Saturn's C ring on 62 stellar occultation profiles. These profiles were obtained by Cassini's Ultraviolet Imaging Spectrograph High Speed Photometer. We used a WWZ wavelet power transform to analyze them. With a co-adding process, we found evidence of 40 wavelike structures, 18 of which are reported here for the first time. Seventeen of these appear to be propagating waves (wavelength changing systematically with distance from Saturn). The longest new wavetrain in the C ring is a 52-km-long wave in a plateau at 86,397 km. We produced a complete map of resonances with external satellites and possible structures rotating with Saturn's rotation period up to the eighth order, allowing us to associate a previously observed wave with the Atlas 2:1 inner Lindblad resonance (ILR) and newly detected waves with the Mimas 6:2 ILR and the Pandora 4:2 ILR. We derived surface mass densities and mass extinction coefficients, finding sigma = 0.22(+/- 0.03) g cm(-2) for the Atlas 2:1 ILR, sigma = 1.31(+/- 0.20) g cm(-2) for the Mimas 6:2 ILR, and sigma = 1.42(+/- 0.21) g cm(-2) for the Pandora 4:2 ILR. We determined a range of mass extinction coefficients (kappa = tau/sigma) for the waves associated with resonances with kappa = 0.13 (+/- 0.03) to 0.28(+/- 0.06) cm(2) g(-1), where tau is the optical depth. These values are higher than the reported values for the A ring (0.01-0.02 cm(2) g(-1)) and the Cassini Division (0.07-0.12 cm(2) g(-1) from Colwell et al. (Colwell, J.E., Cooney, J.H., Esposito, LW., Sremcevic, M. [2009]. Icarus 200, 574-580)). We also note that the mass extinction coefficient is probably not constant across the C ring (in contrast to the A ring and the Cassini Division): it is systematically higher in the plateaus than elsewhere, suggesting smaller particles in the plateaus. We present the results of our analysis of these waves in the C ring and estimate the mass of the C ring to be between3.7(+/- 0.9) x 10(16) kg and 7.9(+/- 2.0) x 10(16) kg (equivalent to an icy satellite of radius between 28.0(+/- 2.3) km and 36.2(+/- 3.0) km with a density of 400 kg m(-3), close to that of Pan or Atlas). Using the ring viscosity derived from the wave damping length, we also estimate the vertical thickness of the C ring between 1.9(+/- 0.4) m and 5.6(+/- 1.4) m, comparable to the vertical thickness of the Cassini Division. (C) 2011 Published by Elsevier Inc.
C1 [Baillie, Kevin; Colwell, Joshua E.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
   [Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
   [Esposito, Larry W.; Sremcevic, Miodrag] Univ Colorado, LASP, Boulder, CO 80309 USA.
RP Baillie, K (reprint author), Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
EM kevin.baillie@univ-paris-diderot.fr
FU National Aeronautics and Space Administration [NNX10AF20G]
FX This material is based upon work supported by the National Aeronautics
   and Space Administration under Grant No. NNX10AF20G issued through the
   Cassini Data Analysis Program. We are indebted to J.N. Spitale and M.S.
   Tiscareno for valuable suggestions and thorough reviews that improved
   the quality of the manuscript significantly. We also thank J.H. Cooney
   and T. Becker for their helpful comments.
NR 36
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 292
EP 308
DI 10.1016/j.icarus.2011.05.019
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100027
ER

PT J
AU Cloutis, EA
   Hudon, P
   Hiroi, T
   Gaffey, MJ
   Mann, P
AF Cloutis, E. A.
   Hudon, P.
   Hiroi, T.
   Gaffey, M. J.
   Mann, P.
TI Spectral reflectance properties of carbonaceous chondrites: 2. CM
   chondrites
SO ICARUS
LA English
DT Article
DE Asteroids, Surfaces; Meteorites; Spectroscopy
ID INSOLUBLE ORGANIC-MATTER; LOW-ALBEDO ASTEROIDS; X-RAY-DIFFRACTION;
   AQUEOUS ALTERATION; AMORPHOUS-CARBON; CI CHONDRITES;
   MOSSBAUER-SPECTROSCOPY; MATRIX MINERALOGY; SOLAR-SYSTEM; THERMAL
   METAMORPHISM
AB We have examined the spectral reflectance properties and available modal mineralogies of 39 CM carbonaceous chondrites to determine their range of spectral variability and to diagnose their spectral features. We have also reviewed the published literature on CM mineralogy and subclassification, surveyed the published spectral literature and added new measurements of CM chondrites and relevant end members and mineral mixtures, and measured 11 parameters and searched pair-wise for correlations between all quantities. CM spectra are characterized by overall slopes that can range from modestly blue-sloped to red-sloped, with brighter spectra being generally more red-sloped. Spectral slopes, as measured by the 2.4:0.56 mu m and 2.4 mu m:visible region peak reflectance ratios, range from 0.90 to 2.32, and 0.81 to 2.24, respectively, with values <1 indicating blue-sloped spectra. Matrix-enriched CM spectra can be even more blue-sloped than bulk samples, with ratios as low as 0.85. There is no apparent correlation between spectral slope and grain size for CM chondrite spectra - both fine-grained powders and chips can exhibit blue-sloped spectra. Maximum reflectance across the 0.3-2.5 mu m interval ranges from 2.9% to 20.0%, and from 2.8% to 14.0% at 0.56 mu m. Matrix-enriched CM spectra can be darker than bulk samples, with maximum reflectance as low as 2.1%. CM spectra exhibit nearly ubiquitous absorption bands near 0.7, 0.9, and 1.1 mu m, with depths up to 12%, and, less commonly, absorption bands in other wavelength regions (e.g., 0.4-0.5, 0.65, 2.2 mu m). The depths of the 0.7, 0.9, and 1.1 mu m absorption features vary largely in tandem, suggesting a single cause, specifically serpentine-group phyllosilicates. The generally high Fe content, high phyllosilicate abundance relative to mafic silicates, and dual Fe valence state in CM phyllosilicates, all suggest that the phyllosilicates will exhibit strong absorption bands in the 0.7 mu m region (due to Fe(3+) - Fe(2+) charge transfers), and the 0.9-1.2 mu m region (due to Fe(2+) crystal field transitions), and generally dominate over mafic silicates. CM petrologic subtypes exhibit a positive correlation between degree of aqueous alteration and depth of the 0.7 mu m absorption band. This is consistent with the decrease in fine-grained opaques that accompanies aqueous alteration. There is no consistent relationship between degree of aqueous alteration and evidence for a 0.65 mu m region saponite-group phyllosilicate absorption band. Spectra of different subsamples of a single CM can show large variations in absolute reflectance and overall slope. This is probably due to petrologic variations that likely exist within a single CM chondrite, as duplicate spectra for a single subsample show much less spectral variability. When the full suite of available CM spectra is considered, few clear spectral-compositional trends emerge. This indicates that multiple compositional and physical factors affect absolute reflectance, absorption band depths, and absorption band wavelength positions. Asteroids with reflectance spectra that exhibit absorption features consistent with CM spectra (i.e., absorption bands near 0.7 and 0.9 mu m) include members from multiple taxonomic groups.
   This suggests that on CM parent bodies, aqueous alteration resulted in the consistent production of serpentine-group phyllosilicates, however resulting absolute reflectances and spectral shapes seen in CM reflectance spectra are highly variable, accounting for the presence of phyllosilicate fetures in reflectance spectra of asteroids across diverse taxonomic groups. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Cloutis, E. A.; Mann, P.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
   [Hudon, P.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Off, Houston, TX 77058 USA.
   [Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
   [Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada.
EM e.cloutis@uwinnipeg.ca; pierre.hudon@mcgill.ca;
   takahiro_hiroi@brown.edu; gaffey@space.edu
FU NASA [NNG06GJ31G]
FX We wish to thank the invaluable and generous assistance provided by many
   individuals which made this study possible. We particularly thank Dr.
   Jeffrey Post of the Smithsonian Institution National Museum of Natural
   History and Dr. Linda Reinen of Pomona College for providing a number of
   the mineral samples used in this study, Mr. Neil Ball and Dr. Frank
   Hawthorne of the University of Manitoba for acquisition of XRD data for
   the mineral samples, and Dr. Stanley Mertzman for XRF analysis of the
   mineral samples. The establishment and operation of the Planetary
   Spectrophotometer Facility (PSF) at the University of Winnipeg was made
   possible through the assistance of the Canada Foundation for Innovation,
   the Manitoba Research Innovations Fund, the Canadian Space Agency, the
   Natural Sciences and Engineering Research Council of Canada (NSERC), and
   the University of Winnipeg. The RELAB facility at Brown University is a
   multi-user facility operated with support from NASA Planetary Geology
   and Geophysics Grant NNG06GJ31G, whose support is gratefully
   acknowledged. Finally, our thanks to Alan Rubin and Beth Clark for their
   numerous useful suggestions for improving the readability and utility of
   this paper.
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 309
EP 346
DI 10.1016/j.icarus.2011.09.009
PG 38
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100028
ER

PT J
AU Rivera-Valentin, EG
   Blackburn, DG
   Ulrich, R
AF Rivera-Valentin, Edgard G.
   Blackburn, David G.
   Ulrich, Richard
TI Revisiting the thermal inertia of Iapetus: Clues to the thickness of the
   dark material
SO ICARUS
LA English
DT Article
DE Iapetus; Satellites, Surfaces; Saturn, Satellites
ID WATER-ICE; SURFACE-PROPERTIES; ALBEDO DICHOTOMY; PHOEBE; SATELLITES;
   HYPERION; SATURN; MARS; CONDUCTIVITY; SPECTROMETER
AB The energy balance at the surface of an airless planetary body is strongly influenced by the bolometric Bond albedo and the surface thermal inertia. Both of these values may be calculated through the application of a thermal model to measured surface temperatures. The accuracy of either, though, increases if the value of the other is better constrained. In this study, we used the improved global bolometric Bond albedo map of Iapetus derived from Cassini VIMS and ISS and Voyager ISS data in conjunction with Cassini CIRS temperature data to reevaluate surface thermal inertia across Iapetus. Results showed the thermal inertia of the dark terrain varies between 11 and 14.8 J m(-2) K(-1) s(-1/2) while the light material varies between 15 and 25 J m(-2) K(-1) s(-1/2). Using an approximation to the thermal properties of the dark overburden derived from our thermal inertia results, we can implement our thermal model to provide estimates on the dark material thickness, which was found to lie between 7 cm and 16 cm. In order to develop an accurate global thermal model, a weighted function that approximates the surface thermal inertia across Iapetus was developed and verified via our measurements. The global bolometric Bond albedo map, surface thermal inertia map, and the thermal model are then used to synthesize global temperature maps that may be used to study the stability of volatiles. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Rivera-Valentin, Edgard G.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA.
   [Blackburn, David G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Ulrich, Richard] Univ Arkansas, Dept Chem Engn, Fayetteville, AR 72701 USA.
RP Rivera-Valentin, EG (reprint author), Univ Arkansas, Arkansas Ctr Space & Planetary Sci, 202 Field House Bldg, Fayetteville, AR 72701 USA.
EM eriverav@uark.edu
OI Rivera-Valentin, Edgard/0000-0002-4042-003X
FU NASA
FX The authors would like to thank Bonnie J. Buratti for the idea to pursue
   an advanced thermal study of Iapetus, use of NASA's Jet Propulsion
   Laboratory workspace, moral support, and helpful conversation. A portion
   of this work was sponsored by the NASA Space Grant and conducted at Jet
   Propulsion Laboratory, California Institute of Technology, under
   contract of the National Aeronautics and Space Administration. The
   authors would also like to thank the anonymous reviewers that helped to
   enhance this manuscript.
NR 40
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
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IS 1
BP 347
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PG 12
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SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100029
ER

PT J
AU Minnis, P
   Sun-Mack, S
   Young, DF
   Heck, PW
   Garber, DP
   Chen, Y
   Spangenberg, DA
   Arduini, RF
   Trepte, QZ
   Smith, WL
   Ayers, JK
   Gibson, SC
   Miller, WF
   Hong, G
   Chakrapani, V
   Takano, Y
   Liou, KN
   Xie, Y
   Yang, P
AF Minnis, Patrick
   Sun-Mack, Szedung
   Young, David F.
   Heck, Patrick W.
   Garber, Donald P.
   Chen, Yan
   Spangenberg, Douglas A.
   Arduini, Robert F.
   Trepte, Qing Z.
   Smith, William L., Jr.
   Ayers, J. Kirk
   Gibson, Sharon C.
   Miller, Walter F.
   Hong, Gang
   Chakrapani, Venkatesan
   Takano, Yoshihide
   Liou, Kuo-Nan
   Xie, Yu
   Yang, Ping
TI CERES Edition-2 Cloud Property Retrievals Using TRMM VIRS and Terra and
   Aqua MODIS Data-Part I: Algorithms
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Climate; cloud; cloud remote sensing; Clouds and the Earth's Radiant
   Energy System (CERES); MODerate-resolution Imaging Spectrometer (MODIS);
   Visible and Infrared Scanner (VIRS)
ID ENERGY SYSTEM CERES; LIQUID WATER CLOUDS; DIURNAL VARIABILITY;
   OPTICAL-CONSTANTS; REGIONAL CLOUD; SATELLITE; ICE; CHANNELS; FIRE;
   MICROPHYSICS
AB The National Aeronautics and Space Administration's Clouds and the Earth's Radiant Energy System (CERES) Project was designed to improve our understanding of the relationship between clouds and solar and longwave radiation. This is achieved using satellite broad-band instruments to map the top-of-atmosphere radiation fields with coincident data from satellite narrow-band imagers employed to retrieve the properties of clouds associated with those fields. This paper documents the CERES Edition-2 cloud property retrieval system used to analyze data from the Tropical Rainfall Measuring Mission Visible and Infrared Scanner and by the MODerate-resolution Imaging Spectrometer instruments on board the Terra and Aqua satellites covering the period 1998 through 2007. Two daytime retrieval methods are explained: the Visible Infrared Shortwave-infrared Split-window Technique for snow-free surfaces and the Shortwave-infrared Infrared Near-infrared Technique for snow or ice-covered surfaces. The Shortwave-infrared Infrared Split-window Technique is used for all surfaces at night. These methods, along with the ancillary data and empirical parameterizations of cloud thickness, are used to derive cloud boundaries, phase, optical depth, effective particle size, and condensed/frozen water path at both pixel and CERES footprint levels. Additional information is presented, detailing the potential effects of satellite calibration differences, highlighting methods to compensate for spectral differences and correct for atmospheric absorption and emissivity, and discussing known errors in the code. Because a consistent set of algorithms, auxiliary input, and calibrations across platforms are used, instrument and algorithm-induced changes in the data record are minimized. This facilitates the use of the CERES data products for studying climate-scale trends.
C1 [Minnis, Patrick; Young, David F.; Garber, Donald P.; Smith, William L., Jr.] Natl Aeronaut & Space Adm Langley Res Ctr, Hampton, VA 23681 USA.
   [Sun-Mack, Szedung; Chen, Yan; Spangenberg, Douglas A.; Arduini, Robert F.; Trepte, Qing Z.; Ayers, J. Kirk; Gibson, Sharon C.; Miller, Walter F.; Hong, Gang; Chakrapani, Venkatesan] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
   [Heck, Patrick W.] Univ Wisconsin, Natl Ocean & Atmospher Adm Cooperat Inst Meteorol, Madison, WI 53706 USA.
   [Takano, Yoshihide; Liou, Kuo-Nan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
   [Takano, Yoshihide; Liou, Kuo-Nan] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
   [Xie, Yu; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
RP Minnis, P (reprint author), Natl Aeronaut & Space Adm Langley Res Ctr, Hampton, VA 23681 USA.
EM Patrick.Minnis-1@nasa.gov
RI Yang, Ping/B-4590-2011; Hong, Gang/A-2323-2012; Garber,
   Donald/D-7427-2015; 
OI Garber, Donald/0000-0001-7387-3628
FU National Aeronautics and Space Administration Earth Science Enterprise
   Office through the CERES
FX Manuscript received December 22, 2009; revised January 27, 2011;
   accepted March 23, 2011. Date of publication June 7, 2011; date of
   current version October 28, 2011. This work was supported by the
   National Aeronautics and Space Administration Earth Science Enterprise
   Office through the CERES Project.
NR 58
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD NOV
PY 2011
VL 49
IS 11
BP 4374
EP 4400
DI 10.1109/TGRS.2011.2144601
PN 2
PG 27
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA 851ON
UT WOS:000297280500002
ER

PT J
AU Minnis, P
   Sun-Mack, S
   Chen, Y
   Khaiyer, MM
   Yi, YH
   Ayers, JK
   Brown, RR
   Dong, XQ
   Gibson, SC
   Heck, PW
   Lin, B
   Nordeen, ML
   Nguyen, L
   Palikonda, R
   Smith, WL
   Spangenberg, DA
   Trepte, QZ
   Xi, B
AF Minnis, Patrick
   Sun-Mack, Szedung
   Chen, Yan
   Khaiyer, Mandana M.
   Yi, Yuhong
   Ayers, J. Kirk
   Brown, Ricky R.
   Dong, Xiquan
   Gibson, Sharon C.
   Heck, Patrick W.
   Lin, Bing
   Nordeen, Michele L.
   Louis Nguyen
   Palikonda, Rabindra
   Smith, William L., Jr.
   Spangenberg, Douglas A.
   Trepte, Qing Z.
   Xi, Baike
TI CERES Edition-2 Cloud Property Retrievals Using TRMM VIRS and Terra and
   Aqua MODIS Data-Part II: Examples of Average Results and Comparisons
   With Other Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Climate; cloud; cloud remote sensing; Clouds and the Earth's Radiant
   Energy System (CERES); Moderate Resolution Imaging Spectroradiometer
   (MODIS); Visible and Infrared Scanner (VIRS)
ID RADIATION MEASUREMENT PROGRAM; DROPLET EFFECTIVE RADIUS; LIQUID WATER
   PATH; DIURNAL VARIABILITY; VERTICAL VARIATION; ICE CLOUDS; CLEAR-SKY;
   SATELLITE; PRODUCTS; COLLECTION-5
AB Cloud properties were retrieved by applying the Clouds and Earth's Radiant Energy System (CERES) project Edition-2 algorithms to 3.5 years of Tropical Rainfall Measuring Mission Visible and Infrared Scanner data and 5.5 and 8 years of MODerate Resolution Imaging Spectroradiometer (MODIS) data from Aqua and Terra, respectively. The cloud products are consistent quantitatively from all three imagers; the greatest discrepancies occur over ice-covered surfaces. The retrieved cloud cover (similar to 59%) is divided equally between liquid and ice clouds. Global mean cloud effective heights, optical depth, effective particle sizes, and water paths are 2.5 km, 9.9, 12.9 mu m, and 80 g . m(-2), respectively, for liquid clouds and 8.3 km, 12.7, 52.2 mu m, and 230 g . m(-2) for ice clouds. Cloud droplet effective radius is greater over ocean than land and has a pronounced seasonal cycle over southern oceans. Comparisons with independent measurements from surface sites, the Ice Cloud and Land Elevation Satellite, and the Aqua Advanced Microwave Scanning Radiometer-Earth Observing System are used to evaluate the results. The mean CERES and MODIS Atmosphere Science Team cloud properties have many similarities but exhibit large discrepancies in certain parameters due to differences in the algorithms and the number of unretrieved cloud pixels. Problem areas in the CERES algorithms are identified and discussed.
C1 [Minnis, Patrick; Lin, Bing; Louis Nguyen; Smith, William L., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Sun-Mack, Szedung; Chen, Yan; Khaiyer, Mandana M.; Yi, Yuhong; Ayers, J. Kirk; Brown, Ricky R.; Gibson, Sharon C.; Nordeen, Michele L.; Palikonda, Rabindra; Spangenberg, Douglas A.; Trepte, Qing Z.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
   [Dong, Xiquan; Xi, Baike] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
   [Heck, Patrick W.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA.
RP Minnis, P (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM Patrick.Minnis-1@nasa.gov
RI Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
FU NASA Earth Science Enterprise Office; Ice Cloud and Land Elevation
   Satellite Mission; Environmental Sciences Division of the Department of
   Energy [DE-AI02-07ER64546]
FX Manuscript received February 16, 2010; revised January 28, 2011;
   accepted March 23, 2011. Date of publication June 7, 2011; date of
   current version October 28, 2011. This work was supported in part by the
   NASA Earth Science Enterprise Office through the CERES project, the Ice
   Cloud and Land Elevation Satellite Mission, and by the Environmental
   Sciences Division of the Department of Energy through the Atmospheric
   Radiation Measurement Program Interagency Agreement, DE-AI02-07ER64546.
NR 66
TC 47
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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
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD NOV
PY 2011
VL 49
IS 11
BP 4401
EP 4430
DI 10.1109/TGRS.2011.2144602
PN 2
PG 30
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA 851ON
UT WOS:000297280500003
ER

PT J
AU Martin, RA
AF Martin, Rodney A.
TI A State-Space Approach to Optimal Level-Crossing Prediction for Linear
   Gaussian Processes (vol 56, pg 5083, 2010)
SO IEEE TRANSACTIONS ON INFORMATION THEORY
LA English
DT Correction
C1 [Martin, Rodney A.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
   [Martin, Rodney A.] NASA, Ames Res Ctr, Intelligent Data Understanding Grp, Moffett Field, CA 94035 USA.
RP Martin, RA (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
EM rodney.martin@nasa.gov
NR 1
TC 1
Z9 1
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9448
J9 IEEE T INFORM THEORY
JI IEEE Trans. Inf. Theory
PD NOV
PY 2011
VL 57
IS 11
BP 7658
EP 7658
DI 10.1109/TIT.2011.2160614
PG 1
WC Computer Science, Information Systems; Engineering, Electrical &
   Electronic
SC Computer Science; Engineering
GA 848IV
UT WOS:000297046100034
ER

PT J
AU Cantrell, SA
   Cantrell, JH
AF Cantrell, Sean A.
   Cantrell, John H.
TI Renormalization, resonance bifurcation, and phase contrast in dynamic
   atomic force microscopy
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID TAPPING-MODE; ACOUSTIC MICROSCOPY; ENERGY-DISSIPATION; CANTILEVER;
   VIBRATIONS; CONTACT; SURFACE; TIP
AB Renormalization of the model describing dynamic atomic force microscopy is shown to provide a simple and robust interpretation of cantilever dynamics as a single spring and mass with frequency-dependent cantilever stiffness and damping parameters. Renormalization predicts a bifurcation in the free-space cantilever resonance that leads to the occurrence of multiple stable resonance modes experimentally observed during cantilever-sample "contact." The bifurcation results from the coupling of the cantilever modes via the nonlinearity of the tip-sample interaction force and the running of the cantilever parameters with frequency. The effective interaction force is represented by a polynomial expansion with coefficients F-ij (i, j = 0, 1, 2, ...) that account for cantilever-to-sample energy transfer in a single system model. The effective cantilever spring constant obtained from F-10 and the interaction force energy transfer factor obtained from F-01 are used to show that phase contrast in the linear regime of operation can be expressed in terms of conservative or dissipative force parameters alone when operating in constant amplitude control near the free-space resonance frequency of the cantilever. The model predicts that dissipative force parameters dominate phase contrast at low drive frequencies, while conservative force parameters dominate phase contrast at sufficiently high drive frequencies for appropriate values of F-10. (C) 2011 American Institute of Physics. [doi:10.1063/1.3660745]
C1 [Cantrell, John H.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
   [Cantrell, Sean A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Cantrell, JH (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM scantre2@jhu.edu; john.h.cantrell@nasa.gov
FU U.S. Department of Energy, Washington, DC [DE-SC0001764]
FX S.A.C. thanks the U.S. Department of Energy, Washington, DC, for support
   under Prime Award No. DE-SC0001764.
NR 29
TC 3
Z9 3
U1 1
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
   MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD NOV 1
PY 2011
VL 110
IS 9
AR 094314
DI 10.1063/1.3660745
PG 9
WC Physics, Applied
SC Physics
GA 848OY
UT WOS:000297062100106
ER

PT J
AU Brunke, MA
   Wang, Z
   Zeng, XB
   Bosilovich, M
   Shie, CL
AF Brunke, Michael A.
   Wang, Zhuo
   Zeng, Xubin
   Bosilovich, Michael
   Shie, Chung-Lin
TI An Assessment of the Uncertainties in Ocean Surface Turbulent Fluxes in
   11 Reanalysis, Satellite-Derived, and Combined Global Datasets
SO JOURNAL OF CLIMATE
LA English
DT Article
ID LATENT-HEAT FLUX; AIR-SEA FLUXES; ATMOSPHERE RESPONSE EXPERIMENT; BULK
   AERODYNAMIC ALGORITHMS; RADIATIVE-TRANSFER MODEL; SENSOR MICROWAVE
   IMAGER; DATA SETS; EQUATORIAL PACIFIC; EDDY-CORRELATION; NCEP REANALYSES
AB Ocean surface turbulent fluxes play an important role in the energy and water cycles of the atmosphere-ocean coupled system, and several flux products have become available in recent years. Here, turbulent fluxes from 6 widely used reanalyses, 4 satellite-derived flux products, and 2 combined product are evaluated by comparison with direct covariance latent heat (LH) and sensible heat (SH) fluxes and inertial-dissipation wind stresses measured from 12 cruises over the tropics and mid- and high latitudes. The biases range from -3.0 to 20.2 W m(-2) for LH flux, from -1.4 to 6.0 W m(-2) for SH flux, and from -7.6 to 7.9 x 10(-3) N m(-2) for wind stress. These biases are small for moderate wind speeds but diverge for strong wind speeds (>10 m s(-1)). The total flux biases are then further evaluated by dividing them into uncertainties due to errors in the bulk variables and the residual uncertainty. The bulk-variable-caused uncertainty dominates many products' SH flux and wind stress biases. The biases in the bulk variables that contribute to this uncertainty can be quite high depending on the cruise and the variable. On the basis of a ranking of each product's flux, it is found that the Modern-Era Retrospective Analysis for Research and Applications (MERRA) is among the "best performing" for all three fluxes. Also, the European Centre for Medium-Range Weather Forecasts (ECMWF) interim reanalysis (ERA-Interim) and the National Centers for Environmental Prediction-Department of Energy (NCEP-DOE) reanalysis are among the best performing for two of the three fluxes. Of the satellite-derived products, version 2b of the Goddard Satellite-Based Surface Turbulent Fluxes (GSSTF2b) is among the best performing for two of the three fluxes. Also among the best performing for only one of the fluxes are the 40-yr ERA (ERA-40) and the combined product objectively analyzed air-sea fluxes (OAFlux). Direction for the future development of ocean surface flux datasets is also suggested.
C1 [Brunke, Michael A.; Wang, Zhuo; Zeng, Xubin] Univ Arizona, Dept Atmospher Sci, Tucson, AZ 85721 USA.
   [Bosilovich, Michael] NASA, Goddard Modeling & Assimilat Off, Greenbelt, MD USA.
   [Shie, Chung-Lin] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
   [Shie, Chung-Lin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Brunke, MA (reprint author), Univ Arizona, Dept Atmospher Sci, POB 210081, Tucson, AZ 85721 USA.
EM brunke@atmo.arizona.edu
RI Bosilovich, Michael/F-8175-2012; 
OI Zeng, Xubin/0000-0001-7352-2764
FU NASA [NNX09A021G]
FX This work was supported by NASA under Grant NNX09A021G. Dr. C. Fairall
   is thanked for providing the ship cruise data and the COARE 3.0
   algorithm used here. We also thank Drs. A. Beljaars, H.-L. Pan, and
   S.-H. Chou for providing their algorithms. Dr. A. Beljaars and two
   anonymous reviewers are also thanked for their helpful comments.
   Finally, NCAR is thanked for providing the computing resources to
   download the reanalysis data used here.
NR 81
TC 38
Z9 40
U1 3
U2 32
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD NOV 1
PY 2011
VL 24
IS 21
BP 5469
EP 5493
DI 10.1175/2011JCLI4223.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 841TE
UT WOS:000296535300001
ER

PT J
AU Sippel, JA
   Braun, SA
   Shie, CL
AF Sippel, Jason A.
   Braun, Scott A.
   Shie, Chung-Lin
TI Environmental Influences on the Strength of Tropical Storm Debby (2006)
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID SAHARAN AIR LAYER; GLOBAL DATA ASSIMILATION; AFRICAN EASTERLY WAVES;
   RESOLUTION COUPLED MODEL; CYCLOGENETIC PROCESSES; NUMERICAL SIMULATIONS;
   FORECAST SYSTEM; SOP-3 NAMMA; OCEAN INTERACTION; NORTH-ATLANTIC
AB This study uses mesoscale ensemble forecasts to compare the magnitude of nonaerosol effects of the Saharan air layer (SAL) with other environmental influences on the intensity of Tropical Storm Debby. Debby was a weak Cape Verde storm that dissipated over the tropical North Atlantic a few days after forming in August 2006. The system has received considerable attention because of its vicinity to the SAL as it struggled to intensify, which has led to speculation that the SAL helped lead to the storm's demise. Statistical correlation is used to better understand why some ensemble members strengthen the pre-Debby wave into a hurricane and others develop only a weak vortex.
   Although the results here suggest that the SAL slowed intensification during the predepression to depression stages, it was not likely responsible for Debby's dissipation. The most obvious SAL-related factor to affect long-term intensity in the ensembles is dry air above 2 km, which delays organization of the low-level vortex. Warm temperatures within the SAL and shear associated with the African easterly jet (AEJ) exhibit a weak, secondary relationship with forecast intensity variability. An important result here is that sensitivity to the dry environmental air depends considerably on cyclone strength, and it becomes insignificant once a tropical storm forms. Furthermore, Debby's most rapid period of intensification coincided with its track over somewhat higher sea surface temperatures, and intensification ended when the storm moved over cooler waters. The results herein suggest that this factor might have affected the storm's intensity more strongly than did any effect of the SAL. Even later, subsequent to the period examined by these ensembles, Debby dissipated under the influence of stronger vertical wind shear from an upper-level trough.
   These results show that the relationship among the SAL, AEJ, and developing tropical cyclones is not as straightforward as has been hypothesized by some recent studies. Ultimately, the nuanced relationship between storm intensity and the SAL shows that much care needs to be taken before drawing conclusions about the effect of the SAL on any particular cyclone. The authors therefore advocate more rigorous future analysis through both idealized and ensemble studies to more fully quantify the effect of the SAL on tropical cyclones in general.
C1 [Sippel, Jason A.; Braun, Scott A.; Shie, Chung-Lin] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Sippel, Jason A.; Shie, Chung-Lin] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Sippel, JA (reprint author), NASA, Atmospheres Lab, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA.
EM jason.sippel@nasa.gov
FU Oak Ridge Associated Universities; NASA
FX The authors are grateful to Zhiyong Meng for help on the ensemble
   simulation and to helpful comments from three anonymous reviewers. Work
   by the first author began under the NASA Post-doctoral Program,
   sponsored by Oak Ridge Associated Universities through a contract with
   NASA and continued while the first author was employed at the Goddard
   Earth Sciences and Technology Center. This work was also supported by
   Dr. Ramesh Kakar at NASA Headquarters with funds from the NASA Hurricane
   Science Research Program. The simulations were conducted on NASA Center
   for Climate Simulation facilities.
NR 50
TC 23
Z9 25
U1 1
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD NOV
PY 2011
VL 68
IS 11
BP 2557
EP 2581
DI 10.1175/2011JAS3648.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 849PY
UT WOS:000297138800005
ER

PT J
AU Suzuki, K
   Stephens, GL
   van den Heever, SC
   Nakajima, TY
AF Suzuki, Kentaroh
   Stephens, Graeme L.
   van den Heever, Susan C.
   Nakajima, Takashi Y.
TI Diagnosis of the Warm Rain Process in Cloud-Resolving Models Using Joint
   CloudSat and MODIS Observations
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID DROPLET EFFECTIVE RADIUS; BOUNDARY-LAYER CLOUDS; PART I; MICROPHYSICS
   PARAMETERIZATION; NUMBER CONCENTRATION; OPTICAL-THICKNESS; GROWTH; RAMS;
   SIMULATIONS; DRIZZLE
AB This study examines the warm rain formation process in global and regional cloud-resolving models. Methodologies developed to analyze CloudSat and Moderate Resolution Imaging Spectroradiometer (MODIS) satellite observations are employed to investigate the cloud-to-precipitation processes and are applied to model results for comparisons with corresponding statistics from the observations. Three precipitation categories of no precipitation, drizzle, and rain are defined according to nonattenuated near-surface radar reflectivity, and their fractional occurrences and the probability of precipitation are investigated as a function of cloud properties such as droplet size, optical thickness, droplet number concentration, and liquid water path. The comparisons reveal how the models are qualitatively similar to, but quantitatively different from, observations in terms of cloud-to-rainwater conversion processes. Statistics from one model reveal a much faster formation of rain than observed, with drizzle occurrence being much less frequent, whereas statistics from the other model illustrate rain formation closer to satellite observations but still faster formation of drizzle water. Vertical profiles of radar reflectivity that are resealed as a function of in-cloud optical depth and classified according to particle size are also compared. The results show that each model indicates systematically faster formation of rain and drizzle, respectively, than observed in vertical profiles although they indicate that the cloud-to-rain transitions are qualitatively similar to observations. These results characterize the model behavior in terms of warm cloud microphysics and then point to a possible area of model improvement for more realistic representation of warm rain formation processes.
C1 [Suzuki, Kentaroh; van den Heever, Susan C.] Colorado Slate Univ, Dept Atmospher Sci, Ft Collins, CO USA.
   [Suzuki, Kentaroh; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Nakajima, Takashi Y.] Tokai Univ, Res & Informat Ctr, Tokyo 151, Japan.
RP Suzuki, K (reprint author), CALTECH, Jet Prop Lab, Mail Stop 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kentaro.suzuki@jpl.nasa.gov
RI Nakajima, Takashi/C-2747-2009; Suzuki, Kentaroh/C-3624-2011; van den
   Heever, Susan/E-8728-2011
OI van den Heever, Susan/0000-0001-9843-3864
FU NASA [NNX07AR11G, NNX09AJ45G]; National Science Foundation
   [ATM-0820557]; Japan Aerospace Exploration Agency (JAXA); MEXT in Japan
   [RR2002]
FX We are grateful to Ralf Bennartz and two anonymous reviewers for their
   invaluable comments that greatly improved this paper. We also
   acknowledge Tristan L'Ecuyer and Norm Wood for fruitful discussions and
   John Haynes, who provided the Quick-Beam code. The Cloud Sat data
   products were provided by Cloud Sat Data Processing Center at
   CIRA/Colorado State University. This study was supported by NASA Grants
   NNX07AR11G and NNX09AJ45G. S. C. van den Heever was supported by the
   National Science Foundation under Grant ATM-0820557. T. Y. Nakajima was
   partly supported by the EarthCARE Science Project (2007-2010) and the
   GCOM-C Science Project (2009-2010) of the Japan Aerospace Exploration
   Agency (JAXA). The NICAM-SPRINTARS simulation was performed on the Earth
   Simulator with financial support of the RR2002 project by MEXT in Japan.
   K. Suzuki also acknowledges Tatsuya Seiki for his help to run the model.
NR 53
TC 26
Z9 26
U1 1
U2 12
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 NOV
PY 2011
VL 68
IS 11
BP 2655
EP 2670
DI 10.1175/JAS-D-10-05026.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 849PY
UT WOS:000297138800010
ER

PT J
AU Cui, HC
   Hao, YL
   Kovtun, M
   Stolc, V
   Deng, XW
   Sakakibara, H
   Kojima, M
AF Cui, Hongchang
   Hao, Yueling
   Kovtun, Mikhail
   Stolc, Viktor
   Deng, Xing-Wang
   Sakakibara, Hitoshi
   Kojima, Mikiko
TI Genome-Wide Direct Target Analysis Reveals a Role for SHORT-ROOT in Root
   Vascular Patterning through Cytokinin Homeostasis
SO PLANT PHYSIOLOGY
LA English
DT Article
ID ARABIDOPSIS ROOT; CELL-DIVISION; INTERCELLULAR MOVEMENT; FOUNDER CELLS;
   AUXIN; GENE; EXPRESSION; INITIATION; SCARECROW; MERISTEM
AB SHORT-ROOT (SHR) is a key regulator of root growth and development in Arabidopsis (Arabidopsis thaliana). Made in the stele, the SHR protein moves into an adjacent cell layer, where it specifies endodermal cell fate; it is also essential for apical meristem maintenance, ground tissue patterning, vascular differentiation, and lateral root formation. Much has been learned about the mechanism by which SHR controls radial patterning, but how it regulates other aspects of root morphogenesis is still unclear. To dissect the SHR developmental pathway, we have determined the genome-wide locations of SHR direct targets using a chromatin immunoprecipitation followed by microarray analysis method. K-means clustering analysis not only identified additional quiescent center-specific SHR targets but also revealed a direct role for SHR in gene regulation in the pericycle and xylem. Using cell type-specific markers, we showed that in shr, the phloem and the phloem-associated pericycle expanded, whereas the xylem and xylem-associated pericycle diminished. Interestingly, we found that cytokinin level was elevated in shr and that exogenous cytokinin conferred a shr-like vascular patterning phenotype in wild-type root. By chromatin immunoprecipitation-polymerase chain reaction and reverse transcription-polymerase chain reaction assays, we showed that SHR regulates cytokinin homeostasis by directly controlling the transcription of cytokinin oxidase 3, a cytokinin catabolism enzyme preferentially expressed in the stele. Finally, overexpression of a cytokinin oxidase in shr alleviated its vascular patterning defect. On the basis of these results, we suggest that one mechanism by which SHR controls vascular patterning is the regulation of cytokinin homeostasis.
C1 [Cui, Hongchang; Hao, Yueling] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA.
   [Kovtun, Mikhail] Duke Univ, Dept Biol, Durham, NC 27708 USA.
   [Kovtun, Mikhail] Duke Univ, Inst Genome Sci & Policy, Ctr Syst Biol, Durham, NC 27708 USA.
   [Stolc, Viktor] NASA, Space Biosci Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Deng, Xing-Wang] Yale Univ, New Haven, CT 06520 USA.
   [Sakakibara, Hitoshi; Kojima, Mikiko] RIKEN, Plant Sci Ctr, Yokohama, Kanagawa 2300045, Japan.
RP Cui, HC (reprint author), Florida State Univ, Dept Biol Sci, B-157, Tallahassee, FL 32306 USA.
EM hcui@bio.fsu.edu
RI Sakakibara, Hitoshi/A-6040-2010; 
OI Sakakibara, Hitoshi/0000-0001-5449-6492; Cui,
   Hongchang/0000-0002-9870-748X
FU Florida State University; National Institutes of Health [R01 043778];
   National Aeronautics and Space Administration (NASA) Center for
   Nanotechnology; NASA; Computing, Information, and Communications
   Technology programs [NAS2-99092]
FX This work was supported by setup funds from Florida State University (to
   H. C.), the National Institutes of Health (grant no. R01 043778 to
   P.N.B.), and the National Aeronautics and Space Administration (NASA)
   Center for Nanotechnology, the NASA Fundamental Biology Program, and the
   Computing, Information, and Communications Technology programs (contract
   no. NAS2-99092 to V.S.).
NR 43
TC 31
Z9 36
U1 3
U2 23
PU AMER SOC PLANT BIOLOGISTS
PI ROCKVILLE
PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA
SN 0032-0889
J9 PLANT PHYSIOL
JI Plant Physiol.
PD NOV
PY 2011
VL 157
IS 3
BP 1221
EP 1231
DI 10.1104/pp.111.183178
PG 11
WC Plant Sciences
SC Plant Sciences
GA 844BL
UT WOS:000296722300021
PM 21951467
ER

PT J
AU Sullivan, RM
   Stokes, EH
   Baker, EH
AF Sullivan, Roy M.
   Stokes, Eric H.
   Baker, Eric H.
TI Effect of Time at Temperature on the Ply-Normal Modulus of Carbon
   Phenolic
SO AIAA JOURNAL
LA English
DT Article
ID GLASS-TRANSITION TEMPERATURE; EPOXY; WATER
AB The effect of heating rate and time at temperature on the ply-normal tensile modulus of carbon cloth phenolic is investigated. The results of previous experimental studies reveal that slower heating rates and longer times at temperature result in a higher tensile modulus. It is speculated that the heating rate effect is due to a combination of moisture diffusion and the effect of water on the glass transition of the phenolic polymer. An equation is proposed that defines the value of the ply-normal modulus as a function of temperature and moisture content. Numerical solutions for moisture diffusion in the ply-normal tensile specimen are performed, and the equation for the ply-normal modulus is applied to calculate the modulus as a function of temperature and heating rate. The numerical results are successful in simulating the measured effect of heating rate and time at temperature on the ply-normal modulus. The validity of the supposition that the heating rate and time at temperature effect is due to the combination of moisture diffusion and plasticization of the phenolic polymer is demonstrated.
C1 [Sullivan, Roy M.] NASA, John H Glenn Res Ctr Lewis Field, Struct & Mat Div, Cleveland, OH 44135 USA.
   [Stokes, Eric H.] So Res Inst, Mat Res Dept, Birmingham, AL 35211 USA.
   [Baker, Eric H.] Connecticut Reserve Technol, Struct & Mat Div, Cleveland, OH 44135 USA.
RP Sullivan, RM (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Struct & Mat Div, 21000 Brookpk Rd,Mail Stop 49-7, Cleveland, OH 44135 USA.
FU NASA
FX The first and third authors are grateful for funding from the Reusable
   Solid Rocket Motor V Project under NASA's Constellation Program. The
   first author is also grateful for funding from the Hypersonics Project
   under NASA's Fundamental Aeronautics Program. The second author
   acknowledges funding from the RSRM Project under NASA's Space Shuttle
   Program.
NR 17
TC 0
Z9 0
U1 2
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 NOV
PY 2011
VL 49
IS 11
BP 2482
EP 2490
DI 10.2514/1.J050960
PG 9
WC Engineering, Aerospace
SC Engineering
GA 845LW
UT WOS:000296825200013
ER

PT J
AU Kelly, S
   Segal, C
   Peugeot, J
AF Kelly, Sean
   Segal, Corin
   Peugeot, John
TI Simulation of Cryogenics Cavitation
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 49th AIAA Aerospace Sciences Meeting/New Horizons Forum and Aerospace
   Exposition
CY JAN 04-07, 2011
CL Orlando, FL
SP AIAA
AB Cavitation in cryogenic fluids was simulated on a NACA 0015 hydrofoil in a closed-loop facility filled with a perfluorinated ketone that exhibits a strong thermodynamic effect at ambient conditions. Static pressures were measured at seven locations along the hydrofoil chord and along the wall of the test section. Speeds up to 7.5 m/s and temperatures up to 40 degrees C showed the formation and collapse of vapor bubbles in regimes ranging from incipient cavitation to supercavitation. Effects of velocity, cavitation number, add temperature were studied. For the two lower inlet temperature cases, cavitation was observed before the local static pressure dropped to the saturation pressure corresponding to the inlet temperature. Pressure and frequency analysis of this phenomenon is described below.
C1 [Kelly, Sean; Segal, Corin] Univ Florida, Gainesville, FL 32611 USA.
   [Peugeot, John] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35811 USA.
RP Kelly, S (reprint author), Univ Florida, MAE-A 231,POB 116250, Gainesville, FL 32611 USA.
NR 12
TC 4
Z9 4
U1 0
U2 6
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD NOV
PY 2011
VL 49
IS 11
BP 2502
EP 2510
DI 10.2514/1.J051033
PG 9
WC Engineering, Aerospace
SC Engineering
GA 845LW
UT WOS:000296825200015
ER

PT J
AU Afsar, MZ
   Goldstein, ME
   Fagan, A
AF Afsar, M. Z.
   Goldstein, M. E.
   Fagan, A.
TI Enthalpy-Flux/Momentum-Flux Coupling in the Acoustic Spectrum of Heated
   Jets
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 SCALING LAWS; MIXING NOISE; HOT JETS; TEMPERATURE; TURBULENCE; VELOCITY;
   AEROACOUSTICS; SCATTERING; RAYLEIGH; DENSITY
AB Exhaust flows from aircraft engines operate at higher temperatures than those of the freestream. Accurate predictions of jet noise in heated flows is therefore of considerable interest. In this paper, a self-consistent jet noise model in heated flows is developed using the generalized acoustic analogy. To begin with, it is demonstrated that the exact acoustic spectrum can be written as the sum of three terms: the momentum-flux autocovariance term, the enthalpy-flux/momentum-flux covariance (or the coupling term), and the enthalpy-flux autocovariance. By extending an axisymmetric turbulence model to heated-jet flows, it is shown that the number of independent components in the acoustic spectrum can be reduced to 11 terms. The paper then focuses on the structure of the coupling term using recent Rayleigh scattering measurements in heated flows taken at NASA John H. Glenn Research Center at Lewis Field. It is shown that the coupling term becomes increasingly important as the acoustic Mach number increases. That is, it can provide either enhancement or cancellation to the acoustic spectrum, depending on the acoustic Mach number and the position of the observation point. This behavior can help explain why heating reduces the overall sound pressure level at all observation angles in supersonic jets.
C1 [Afsar, M. Z.; Goldstein, M. E.; Fagan, A.] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
RP Afsar, MZ (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
EM mohammed.afsar@cantab.net
NR 57
TC 1
Z9 1
U1 0
U2 5
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD NOV
PY 2011
VL 49
IS 11
BP 2522
EP 2531
DI 10.2514/1.J051076
PG 10
WC Engineering, Aerospace
SC Engineering
GA 845LW
UT WOS:000296825200017
ER

PT J
AU Abazajian, KN
   Calabrese, E
   Cooray, A
   De Bernardis, F
   Dodelson, S
   Friedland, A
   Fuller, GM
   Hannestad, S
   Keating, BG
   Linder, EV
   Lunardini, C
   Melchiorri, A
   Miquel, R
   Pierpaoli, E
   Pritchard, J
   Serra, P
   Takada, M
   Wong, YYY
AF Abazajian, K. N.
   Calabrese, E.
   Cooray, A.
   De Bernardis, F.
   Dodelson, S.
   Friedland, A.
   Fuller, G. M.
   Hannestad, S.
   Keating, B. G.
   Linder, E. V.
   Lunardini, C.
   Melchiorri, A.
   Miquel, R.
   Pierpaoli, E.
   Pritchard, J.
   Serra, P.
   Takada, M.
   Wong, Y. Y. Y.
TI Cosmological and astrophysical neutrino mass measurements
SO ASTROPARTICLE PHYSICS
LA English
DT Review
DE Neutrinos; Cosmology
ID LYMAN-ALPHA FOREST; DIGITAL SKY SURVEY; EQUATION-OF-STATE; POWER
   SPECTRUM; CONCORDANCE MODEL; PRESSURE SUPPORT; DARK-MATTER; PARAMETERS;
   REIONIZATION; SIMULATIONS
AB Cosmological and astrophysical measurements provide powerful constraints on neutrino masses complementary to those from accelerators and reactors. Here we provide a guide to these different probes, for each explaining its physical basis, underlying assumptions, current and future reach. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Dodelson, S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
   [Abazajian, K. N.] Univ Maryland, Dept Phys, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.
   [Calabrese, E.; Melchiorri, A.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
   [Calabrese, E.; Melchiorri, A.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, I-00185 Rome, Italy.
   [Cooray, A.; De Bernardis, F.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Dodelson, S.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
   [Dodelson, S.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
   [Friedland, A.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
   [Fuller, G. M.; Keating, B. G.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
   [Hannestad, S.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
   [Linder, E. V.] Berkeley Lab, Berkeley, CA 94720 USA.
   [Linder, E. V.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
   [Linder, E. V.] Ewha Womans Univ, Inst Early Universe WCU, Seoul, South Korea.
   [Lunardini, C.] Arizona State Univ, Tempe, AZ 85287 USA.
   [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
   [Miquel, R.] Inst Fis Altes Energies, E-08193 Bellaterra, Barcelona, Spain.
   [Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
   [Pritchard, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Serra, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Takada, M.] Univ Tokyo, IPMU, Chiba 2778582, Japan.
   [Wong, Y. Y. Y.] Rhein Westfal TH Aachen, Inst Theoret Teilchenphys & Kosmol, D-52056 Aachen, Germany.
RP Dodelson, S (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM Dodelson@fnal.gov
RI Takada, Masahiro/A-4364-2011; Serra, Paolo/G-9678-2014; 
OI Serra, Paolo/0000-0002-7609-3931; Melchiorri,
   Alessandro/0000-0001-5326-6003; Pritchard, Jonathan/0000-0003-4127-5353;
   Miquel, Ramon/0000-0002-6610-4836; Pierpaoli, Elena/0000-0002-7957-8993
NR 81
TC 85
Z9 85
U1 0
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD NOV
PY 2011
VL 35
IS 4
BP 177
EP 184
DI 10.1016/j.astropartphys.2011.07.002
PG 8
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 846XU
UT WOS:000296937300003
ER

PT J
AU Calvez, A
   Essey, W
   Fairbairn, M
   Kusenko, A
   Loewenstein, M
AF Calvez, Antoine
   Essey, Warren
   Fairbairn, Malcolm
   Kusenko, Alexander
   Loewenstein, Michael
TI On the use of X-ray and gamma-ray telescopes for identifying the origin
   of electrons and positrons observed by ATIC, Fermi, and PAMELA
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Dark matter; X-ray observations; Indirect detection of dark matter
ID DWARF SPHEROIDAL GALAXIES; DARK-MATTER; COSMIC-RAY; MAGNETIC-FIELDS;
   CONSTRAINTS; ENERGIES; CLUSTERS; SEARCH; HALOS; DRACO
AB X-ray and gamma-ray observations can help understand the origin of the electron and positron signals reported by ATIC, PAMELA, PPB-BETS, and Fermi. It remains unclear whether the observed high-energy electrons and positrons are produced by relic particles, or by some astrophysical sources. To distinguish between the two possibilities, one can compare the electron population in the local neighborhood with that in the dwarf spheroidal galaxies, which are not expected to host as many pulsars and other astrophysical sources. This can be accomplished using X-ray and gamma-ray observations of dwarf spheroidal galaxies. Assuming the signal detected by Fermi and ATIC comes from dark matter and using the inferred dark matter profile of the Draco dwarf spheroidal galaxy as an example, we calculate the photon spectrum produced by electrons via inverse Compton scattering. Since little is known about the magnetic fields in dwarf spheroidal galaxies, we consider the propagation of charged particles with and without diffusion. Extending the analysis of Fermi collaboration for Draco, we find that for a halo mass similar to 10(9) M., even in the absence of diffusion, the;gamma-ray signal would be above the upper limits. This conclusion is subject to uncertainties associated with the halo mass. If dwarf spheroidal galaxies host local magnetic fields, the diffusion of the electrons can result in a signal detectable by future X-ray telescopes. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Calvez, Antoine; Essey, Warren; Kusenko, Alexander] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [Fairbairn, Malcolm] Kings Coll London, Dept Phys, London WC2R 2LS, England.
   [Kusenko, Alexander] Univ Tokyo, IPMU, Chiba 2778568, Japan.
   [Loewenstein, Michael] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Loewenstein, Michael] CRESST, Greenbelt, MD USA.
   [Loewenstein, Michael] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD USA.
RP Kusenko, A (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
EM kusenko@ucla.edu
FU DOE [DE-FG03-91ER40662]; NASA [NNX08AL48G, NNX11AD36G]; EU Marie Curie
   Network UniverseNet [HPRN-CT-2006-035863]
FX We thank the Astro-H team for providing simulation tools. A.K. thanks P.
   Biermann for helpful comments. The work of A.C. and A.K. was supported
   in part by DOE grant DE-FG03-91ER40662 and by the NASA ATP grant
   NNX08AL48G. M.L. was supported by NASA ADAP grant NNX11AD36G. M.F.
   acknowledges support from the EU Marie Curie Network UniverseNet
   (HPRN-CT-2006-035863).
NR 55
TC 2
Z9 2
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD NOV
PY 2011
VL 35
IS 4
BP 185
EP 191
DI 10.1016/j.astropartphys.2011.07.005
PG 7
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 846XU
UT WOS:000296937300004
ER

PT J
AU Buchhave, LA
   Latham, DW
   Carter, JA
   Desert, JM
   Torres, G
   Adams, ER
   Bryson, ST
   Charbonneau, DB
   Ciardi, DR
   Kulesa, C
   Dupree, AK
   Fischer, DA
   Fressin, F
   Gautier, TN
   Gilliland, RL
   Howell, SB
   Isaacson, H
   Jenkins, JM
   Marcy, GW
   McCarthy, DW
   Rowe, JF
   Batalha, NM
   Borucki, WJ
   Brown, TM
   Caldwell, DA
   Christiansen, JL
   Cochran, WD
   Deming, D
   Dunham, EW
   Everett, M
   Ford, EB
   Fortney, JJ
   Geary, JC
   Girouard, FR
   Haas, MR
   Holman, MJ
   Horch, E
   Klaus, TC
   Knutson, HA
   Koch, DG
   Kolodziejczak, J
   Lissauer, JJ
   Machalek, P
   Mullally, F
   Still, MD
   Quinn, SN
   Seager, S
   Thompson, SE
   Van Cleve, J
AF Buchhave, Lars A.
   Latham, David W.
   Carter, Joshua A.
   Desert, Jean-Michel
   Torres, Guillermo
   Adams, Elisabeth R.
   Bryson, Stephen T.
   Charbonneau, David B.
   Ciardi, David R.
   Kulesa, Craig
   Dupree, Andrea K.
   Fischer, Debra A.
   Fressin, Francois
   Gautier, Thomas N., III
   Gilliland, Ronald L.
   Howell, Steve B.
   Isaacson, Howard
   Jenkins, Jon M.
   Marcy, Geoffrey W.
   McCarthy, Donald W.
   Rowe, Jason F.
   Batalha, Natalie M.
   Borucki, William J.
   Brown, Timothy M.
   Caldwell, Douglas A.
   Christiansen, Jessie L.
   Cochran, William D.
   Deming, Drake
   Dunham, Edward W.
   Everett, Mark
   Ford, Eric B.
   Fortney, Jonathan J.
   Geary, John C.
   Girouard, Forrest R.
   Haas, Michael R.
   Holman, Matthew J.
   Horch, Elliott
   Klaus, Todd C.
   Knutson, Heather A.
   Koch, David G.
   Kolodziejczak, Jeffrey
   Lissauer, Jack J.
   Machalek, Pavel
   Mullally, Fergal
   Still, Martin D.
   Quinn, Samuel N.
   Seager, Sara
   Thompson, Susan E.
   Van Cleve, Jeffrey
TI KEPLER-14b: A MASSIVE HOT JUPITER TRANSITING AN F STAR IN A CLOSE VISUAL
   BINARY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planetary systems; stars: individual (Kepler-14b, KIC 10264660, 2MASS
   J19105011+4719589); techniques: photometric; techniques: spectroscopic
ID SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; EXTRASOLAR PLANET;
   K-DWARF; STELLAR; MISSION; II.; PARAMETERS; ATMOSPHERE; DISCOVERY
AB We present the discovery of a hot Jupiter transiting an F star in a close visual (0 ''.3 sky projected angular separation) binary system. The dilution of the host star's light by the nearly equal magnitude stellar companion (similar to 0.5 mag fainter) significantly affects the derived planetary parameters, and if left uncorrected, leads to an underestimate of the radius and mass of the planet by 10% and 60%, respectively. Other published exoplanets, which have not been observed with high-resolution imaging, could similarly have unresolved stellar companions and thus have incorrectly derived planetary parameters. Kepler-14b (KOI-98) has a period of P = 6.790 days and, correcting for the dilution, has a mass of M-p = 8.40(-0.34)(+ 0.35) M-J and a radius of R-p = 1.136(-0.054)(+ 0.073) R-J, yielding a mean density of rho(p) = 7.1 +/- 1.1 g cm(-3).
C1 [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
   [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
   [Latham, David W.; Carter, Joshua A.; Desert, Jean-Michel; Torres, Guillermo; Adams, Elisabeth R.; Charbonneau, David B.; Dupree, Andrea K.; Fressin, Francois; Geary, John C.; Holman, Matthew J.; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91109 USA.
   [Kulesa, Craig] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
   [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
   [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Isaacson, Howard; Marcy, Geoffrey W.; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Jenkins, Jon M.; Rowe, Jason F.; Caldwell, Douglas A.; Christiansen, Jessie L.; Machalek, Pavel; Mullally, Fergal; Thompson, Susan E.; Van Cleve, Jeffrey] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [McCarthy, Donald W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA.
   [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
   [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
   [Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
   [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
   [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
   [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Girouard, Forrest R.; Klaus, Todd C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
   [Kolodziejczak, Jeffrey] MSFC, Huntsville, AL 35805 USA.
   [Still, Martin D.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Seager, Sara] MIT, Newton, MA 02159 USA.
RP Buchhave, LA (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark.
RI Carter, Joshua/A-8280-2013; Caldwell, Douglas/L-7911-2014; 
OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
   David/0000-0002-5741-3047; Caldwell, Douglas/0000-0003-1963-9616;
   /0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861; Fortney,
   Jonathan/0000-0002-9843-4354
FU Carlsberg Foundation; NASA's Science Mission Directorate; NASA; NASA
   through JPL/Caltech
FX The work of L.A.B. was supported by the Carlsberg Foundation. Funding
   for this Discovery Mission is provided by NASA's Science Mission
   Directorate. This paper uses observations obtained with the Nordic
   Optical Telescope, operated on the island of La Palma jointly by
   Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish
   Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
   de Canarias. This work is also based on observations made with the
   Spitzer Space Telescope which is operated by the Jet Propulsion
   Laboratory, California Institute of Technology under a contract with
   NASA. Support for this work was also provided by NASA through an award
   issued by JPL/Caltech.
NR 37
TC 35
Z9 35
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 NOV
PY 2011
VL 197
IS 1
AR 3
DI 10.1088/0067-0049/197/1/3
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400003
ER

PT J
AU Cochran, WD
   Fabrycky, DC
   Torres, G
   Fressin, F
   Desert, JM
   Ragozzine, D
   Sasselov, D
   Fortney, JJ
   Rowe, JF
   Brugamyer, EJ
   Bryson, ST
   Carter, JA
   Ciardi, DR
   Howell, SB
   Steffen, JH
   Borucki, WJ
   Koch, DG
   Winn, JN
   Welsh, WF
   Uddin, K
   Tenenbaum, P
   Still, M
   Seager, S
   Quinn, SN
   Mullally, F
   Miller, N
   Marcy, GW
   MacQueen, PJ
   Lucas, P
   Lissauer, JJ
   Latham, DW
   Knutson, H
   Kinemuchi, K
   Johnson, JA
   Jenkins, JM
   Isaacson, H
   Howard, A
   Horch, E
   Holman, MJ
   Henze, CE
   Haas, MR
   Gilliland, RL
   Gautier, TN
   Ford, EB
   Fischer, DA
   Everett, M
   Endl, M
   Demory, BO
   Deming, D
   Charbonneau, D
   Caldwell, D
   Buchhave, L
   Brown, TM
   Batalha, N
AF Cochran, William D.
   Fabrycky, Daniel C.
   Torres, Guillermo
   Fressin, Francois
   Desert, Jean-Michel
   Ragozzine, Darin
   Sasselov, Dimitar
   Fortney, Jonathan J.
   Rowe, Jason F.
   Brugamyer, Erik J.
   Bryson, Stephen T.
   Carter, Joshua A.
   Ciardi, David R.
   Howell, Steve B.
   Steffen, Jason H.
   Borucki, William. J.
   Koch, David G.
   Winn, Joshua N.
   Welsh, William F.
   Uddin, Kamal
   Tenenbaum, Peter
   Still, M.
   Seager, Sara
   Quinn, Samuel N.
   Mullally, F.
   Miller, Neil
   Marcy, Geoffrey W.
   MacQueen, Phillip J.
   Lucas, Phillip
   Lissauer, Jack J.
   Latham, David W.
   Knutson, Heather
   Kinemuchi, K.
   Johnson, John A.
   Jenkins, Jon M.
   Isaacson, Howard
   Howard, Andrew
   Horch, Elliott
   Holman, Matthew J.
   Henze, Christopher E.
   Haas, Michael R.
   Gilliland, Ronald L.
   Gautier, Thomas N., III
   Ford, Eric B.
   Fischer, Debra A.
   Everett, Mark
   Endl, Michael
   Demory, Brice-Oliver
   Deming, Drake
   Charbonneau, David
   Caldwell, Douglas
   Buchhave, Lars
   Brown, Timothy M.
   Batalha, Natalie
TI KEPLER-18b, c, AND d: A SYSTEM OF THREE PLANETS CONFIRMED BY TRANSIT
   TIMING VARIATIONS, LIGHT CURVE VALIDATION, WARM-SPITZER PHOTOMETRY, AND
   RADIAL VELOCITY MEASUREMENTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planetary systems; stars: individual (Kepler-18, KIC 8644288, 2MASS
   J19521906+4444467); techniques: photometric; techniques: spectroscopic
ID EXOPLANET HD 189733B; SOLAR-TYPE STARS; LOW-DENSITY; INITIAL
   CHARACTERISTICS; TERRESTRIAL PLANETS; SECONDARY ECLIPSE;
   SPACE-TELESCOPE; BLEND SCENARIOS; TARGET STARS; SUPER-EARTHS
AB We report the detection of three transiting planets around a Sun-like star, which we designate Kepler-18. The transit signals were detected in photometric data from the Kepler satellite, and were confirmed to arise from planets using a combination of large transit-timing variations (TTVs), radial velocity variations, Warm-Spitzer observations, and statistical analysis of false-positive probabilities. The Kepler-18 star has a mass of 0.97M(circle dot), a radius of 1.1R(circle dot), an effective temperature of 5345 K, and an iron abundance of [Fe/H] = +0.19. The planets have orbital periods of approximately 3.5, 7.6, and 14.9 days. The innermost planet "b" is a "super-Earth" with a mass of 6.9 +/- 3.4M(circle plus), a radius of 2.00 +/- 0.10R(circle plus), and a mean density of 4.9 +/- 2.4 g cm(3). The two outer planets "c" and "d" are both low-density Neptune-mass planets. Kepler-18c has a mass of 17.3 +/- 1.9 M-circle plus, a radius of 5.49 +/- 0.26R(circle plus), and a mean density of 0.59 +/- 0.07 g cm(3), while Kepler-18d has a mass of 16.4 +/- 1.4 M-circle plus, a radius of 6.98 +/- 0.33 R-circle plus and a mean density of 0.27 +/- 0.03 g cm(.)(3) Kepler-18c and Kepler-18d have orbital periods near a 2:1 mean-motion resonance, leading to large and readily detected TTVs.
C1 [Cochran, William D.; MacQueen, Phillip J.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
   [Fabrycky, Daniel C.; Fortney, Jonathan J.; Miller, Neil] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Torres, Guillermo; Fressin, Francois; Desert, Jean-Michel; Ragozzine, Darin; Sasselov, Dimitar; Carter, Joshua A.; Quinn, Samuel N.; Latham, David W.; Holman, Matthew J.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Brugamyer, Erik J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
   [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
   [Winn, Joshua N.; Seager, Sara; Demory, Brice-Oliver] MIT, Dept Phys, Cambridge, MA 02139 USA.
   [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
   [Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Tenenbaum, Peter; Mullally, F.; Jenkins, Jon M.; Caldwell, Douglas] ETI Inst, Mountain View, CA 94043 USA.
   [Still, M.; Kinemuchi, K.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Marcy, Geoffrey W.; Knutson, Heather; Isaacson, Howard; Howard, Andrew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Lucas, Phillip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Johnson, John A.] CALTECH, Dept Astron, Pasadena, CA 91109 USA.
   [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
   [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
   [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
   [Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Buchhave, Lars] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
   [Buchhave, Lars] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
   [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
   [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
RP Cochran, WD (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
EM wdc@astro.as.utexas.edu; jdesert@cfa.harvard.edu; jwinn@mit.edu;
   wfw@kublai.sdsu.edu; kamal.uddin@nasa.gov; Peter.Tenenbaum@nasa.gov;
   martin.d.still@nasa.gov; seager@mit.edu; fergal.mullally@nasa.gov;
   Karen.Kinemuchi@nasa.gov; johnjohn@astro.caltech.edu;
   jjenkins@mail.arc.nasa.gov; horche2@southernct.edu; eford@astro.ufl.edu;
   debra.fischer@gmail.com; Douglas.A.Caldwell@nasa.gov;
   natalie.m.batalha@nasa.gov
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell,
   Douglas/L-7911-2014; Howard, Andrew/D-4148-2015
OI Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars
   A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Demory,
   Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Fischer,
   Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183;
   Caldwell, Douglas/0000-0003-1963-9616; Howard,
   Andrew/0000-0001-8638-0320
FU NASA's Science Mission Directorate; NASA through JPL/Caltech; W. M. Keck
   Foundation; NASA
FX Kepler was competitively selected as the tenth Discovery mission.
   Funding for the Kepler Mission is provided by NASA's Science Mission
   Directorate. We are deeply grateful for the very hard work of the entire
   Kepler team. This research 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. Some of the data presented herein were obtained at the
   W. M. Keck Observatory, which is operated as a scientific partnership
   among the California Institute of Technology, the University of
   California, and the National Aeronautics and Space Administration. The
   Keck Observatory was made possible by the generous financial support of
   the W. M. Keck Foundation.
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ER

PT J
AU Desert, JM
   Charbonneau, D
   Demory, BO
   Ballard, S
   Carter, JA
   Fortney, JJ
   Cochran, WD
   Endl, M
   Quinn, SN
   Isaacson, HT
   Fressin, F
   Buchhave, LA
   Latham, DW
   Knutson, HA
   Bryson, ST
   Torres, G
   Rowe, JF
   Batalha, NM
   Borucki, WJ
   Brown, TM
   Caldwell, DA
   Christiansen, JL
   Deming, D
   Fabrycky, DC
   Ford, EB
   Gilliland, RL
   Gillon, M
   Haas, MR
   Jenkins, JM
   Kinemuchi, K
   Koch, D
   Lissauer, JJ
   Lucas, P
   Mullally, F
   MacQueen, PJ
   Marcy, GW
   Sasselov, DD
   Seager, S
   Still, M
   Tenenbaum, P
   Uddin, K
   Winn, JN
AF Desert, Jean-Michel
   Charbonneau, David
   Demory, Brice-Olivier
   Ballard, Sarah
   Carter, Joshua A.
   Fortney, Jonathan J.
   Cochran, William D.
   Endl, Michael
   Quinn, Samuel N.
   Isaacson, Howard T.
   Fressin, Francois
   Buchhave, Lars A.
   Latham, David W.
   Knutson, Heather A.
   Bryson, Stephen T.
   Torres, Guillermo
   Rowe, Jason F.
   Batalha, Natalie M.
   Borucki, William J.
   Brown, Timothy M.
   Caldwell, Douglas A.
   Christiansen, Jessie L.
   Deming, Drake
   Fabrycky, Daniel C.
   Ford, Eric B.
   Gilliland, Ronald L.
   Gillon, Michael
   Haas, Michael R.
   Jenkins, Jon M.
   Kinemuchi, Karen
   Koch, David
   Lissauer, Jack J.
   Lucas, Philip
   Mullally, Fergal
   MacQueen, Phillip J.
   Marcy, Geoffrey W.
   Sasselov, Dimitar D.
   Seager, Sara
   Still, Martin
   Tenenbaum, Peter
   Uddin, Kamal
   Winn, Joshua N.
TI THE HOT-JUPITER KEPLER-17b: DISCOVERY, OBLIQUITY FROM STROBOSCOPIC
   STARSPOTS, AND ATMOSPHERIC CHARACTERIZATION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE eclipses; planetary systems; stars: individual (Kepler-17b, KIC
   10619192, 2MASS 19533486+4748540); techniques: photometric
ID EXTRASOLAR GIANT PLANETS; TRANSIT LIGHT-CURVE; HOBBY-EBERLY TELESCOPE;
   SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; INITIAL CHARACTERISTICS;
   SECONDARY ECLIPSE; THERMAL EMISSION; STELLAR ACTIVITY; SPECTRAL MODELS
AB This paper reports the discovery and characterization of the transiting hot giant exoplanet Kepler-17b. The planet has an orbital period of 1.486 days, and radial velocity measurements from the Hobby-Eberly Telescope show a Doppler signal of 419.5(-15.6)(+13.3) m s(-1). From a transit-based estimate of the host star's mean density, combined with an estimate of the stellar effective temperature T-eff = 5630 +/- 100 from high-resolution spectra, we infer a stellar host mass of 1.06 +/- 0.07 M-circle dot and a stellar radius of 1.02 +/- 0.03 R-circle dot. We estimate the planet mass and radius to be M-P = 2.45 +/- 0.11 M-J and R-P = 1.31 +/- 0.02 R-J. The host star is active, with dark spots that are frequently occulted by the planet. The continuous monitoring of the star reveals a stellar rotation period of 11.89 days, eight times the planet's orbital period; this period ratio produces stroboscopic effects on the occulted starspots. The temporal pattern of these spot-crossing events shows that the planet's orbit is prograde and the star's obliquity is smaller than 15 degrees. We detected planetary occultations of Kepler-17b with both the Kepler and Spitzer Space Telescopes. We use these observations to constrain the eccentricity, e, and find that it is consistent with a circular orbit (e < 0.011). The brightness temperatures of the planet's infrared bandpasses are T-3.6 mu m = 1880 +/- 100 K and T-4.5 mu m = 1770 +/- 150 K. We measure the optical geometric albedo A(g) in the Kepler bandpass and find A(g) = 0.10 +/- 0.02. The observations are best described by atmospheric models for which most of the incident energy is re-radiated away from the day side.
C1 [Desert, Jean-Michel; Charbonneau, David; Ballard, Sarah; Carter, Joshua A.; Quinn, Samuel N.; Fressin, Francois; Latham, David W.; Torres, Guillermo; Lissauer, Jack J.; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Demory, Brice-Olivier; Seager, Sara; Winn, Joshua N.] MIT, Cambridge, MA 02159 USA.
   [Fortney, Jonathan J.; Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
   [Isaacson, Howard T.; Knutson, Heather A.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
   [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA.
   [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
   [Caldwell, Douglas A.; Jenkins, Jon M.; Mullally, Fergal; Tenenbaum, Peter] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
   [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
   [Kinemuchi, Karen; Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Lucas, Philip] Univ Hertfordshire, Ctr Astrophyiscs Res, Hatfield AL10 9AB, Herts, England.
   [Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Desert, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jdesert@cfa.harvard.edu
RI Carter, Joshua/A-8280-2013; Caldwell, Douglas/L-7911-2014; 
OI Caldwell, Douglas/0000-0003-1963-9616; Fortney,
   Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666;
   Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X;
   Fabrycky, Daniel/0000-0003-3750-0183
FU NASA; NASA through JPL/Caltech; W. M. Keck Foundation
FX This work is also based on observations made with the Spitzer Space
   Telescope, which is operated by the Jet Propulsion Laboratory,
   California Institute of Technology under a contract with NASA. Support
   for this work was provided by NASA through an award issued by
   JPL/Caltech.; Some of the data presented herein were obtained at the W.
   M. Keck Observatory, which is operated as a scientific partnership among
   the California Institute of Technology, the University of California and
   the National Aeronautics and Space Administration. The Observatory was
   made possible by the generous financial support of the W. M. Keck
   Foundation.
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PT J
AU Desert, JM
   Charbonneau, D
   Fortney, JJ
   Madhusudhan, N
   Knutson, HA
   Fressin, F
   Deming, D
   Borucki, WJ
   Brown, TM
   Caldwell, D
   Ford, EB
   Gilliland, RL
   Latham, DW
   Marcy, GW
   Seager, S
AF Desert, Jean-Michel
   Charbonneau, David
   Fortney, Jonathan J.
   Madhusudhan, Nikku
   Knutson, Heather A.
   Fressin, Francois
   Deming, Drake
   Borucki, William J.
   Brown, Timothy M.
   Caldwell, Douglas
   Ford, Eric B.
   Gilliland, Ronald L.
   Latham, David W.
   Marcy, Geoffrey W.
   Seager, Sara
CA Kepler Sci Team
TI THE ATMOSPHERES OF THE HOT-JUPITERS KEPLER-5b AND KEPLER-6b OBSERVED
   DURING OCCULTATIONS WITH WARM-SPITZER AND KEPLER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE eclipses; planetary systems; techniques: photometric
ID EXTRASOLAR GIANT PLANETS; GROUND-BASED DETECTION; INFRARED ARRAY CAMERA;
   EXOPLANET HD 189733B; SECONDARY ECLIPSE; THERMAL EMISSION; LIGHT CURVES;
   INITIAL CHARACTERISTICS; TEMPERATURE INVERSION; THEORETICAL SPECTRA
AB This paper reports the detection and the measurements of occultations of the two transiting hot giant exoplanets Kepler-5b and Kepler-6b by their parent stars. The observations are obtained in the near-infrared with Warm-Spitzer Space Telescope and at optical wavelengths by combining more than a year of Kepler photometry. The investigation consists of constraining the eccentricities of these systems and of obtaining broadband emergent photometric data for individual planets. For both targets, the occultations are detected at the 3 sigma level at each wavelength with midoccultation times consistent with circular orbits. The brightness temperatures of these planets are deduced from the infrared observations and reach T-Spitzer = 1930 +/- 100 K and T-Spitzer = 1660 +/- 120 K for Kepler-5b and Kepler-6b, respectively. We measure optical geometric albedos A(g) in the Kepler bandpass and find A(g) = 0.12 +/- 0.04 for Kepler-5b and A(g) = 0.11 +/- 0.04 for Kepler-6b, leading to upper an limit for the Bond albedo of A(B) <= 0.17 in both cases. The observations for both planets are best described by models for which most of the incident energy is redistributed on the dayside, with only less than 10% of the absorbed stellar flux redistributed to the nightside of these planets.
C1 [Desert, Jean-Michel; Charbonneau, David; Fressin, Francois; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Madhusudhan, Nikku] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
   [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
   [Caldwell, Douglas] SETI Inst, Mountain View, CA 94043 USA.
   [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
   [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley Astron Dept, Berkeley, CA 94720 USA.
   [Seager, Sara] MIT, Newton, MA 02159 USA.
RP Desert, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jdesert@cfa.harvard.edu
RI Kepler, S. O. /H-5901-2012; Caldwell, Douglas/L-7911-2014; 
OI Kepler, S. O. /0000-0002-7470-5703; Caldwell,
   Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354;
   Charbonneau, David/0000-0002-9003-484X; /0000-0001-6545-639X
FU NASA; NASA through JPL/Caltech; NASA's Science Mission Directorate; W.
   M. Keck Foundation
FX We would like to thank Jessie Christiansen, Brice-Olivier Demory, and
   Pavel Machaleck for discussions about Kepler photometry, light curves
   analysis, and interpretation. Thank you to the Spitzer staff at IPAC and
   in particular to Nancy Silbermann for scheduling the observations of
   this large program. We would like to thank Jacob Bean for a variety of
   useful discussions. This work is based on observations made with the
   Spitzer Space Telescope, which is operated by the Jet Propulsion
   Laboratory, California Institute of Technology under a contract with
   NASA. Support for this work was provided by NASA through an award issued
   by JPL/Caltech. This work is also based on observations made with Kepler
   which was competitively selected as the tenth Discovery mission. Funding
   for this mission is provided by NASA's Science Mission Directorate. The
   authors would like to thank the many people who generously gave so much
   their time to make this Mission a success. Some of the data presented
   herein were obtained at the W. M. Keck Observatory, which is
   oper-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.
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PT J
AU Endl, M
   MacQueen, PJ
   Cochran, WD
   Brugamyer, EJ
   Buchhave, LA
   Rowe, J
   Lucas, P
   Isaacson, H
   Bryson, S
   Howell, SB
   Fortney, JJ
   Hansen, T
   Borucki, WJ
   Caldwell, D
   Christiansen, JL
   Ciardi, DR
   Demory, BO
   Everett, M
   Ford, EB
   Haas, MR
   Holman, MJ
   Horch, E
   Jenkins, JM
   Koch, DJ
   Lissauer, JJ
   Machalek, P
   Still, M
   Welsh, WF
   Sanderfer, DT
   Seader, SE
   Smith, JC
   Thompson, SE
   Twicken, JD
AF Endl, Michael
   MacQueen, Phillip J.
   Cochran, William D.
   Brugamyer, Erik J.
   Buchhave, Lars A.
   Rowe, Jason
   Lucas, Phillip
   Isaacson, Howard
   Bryson, Steve
   Howell, Steve B.
   Fortney, Jonathan J.
   Hansen, Terese
   Borucki, William J.
   Caldwell, Douglas
   Christiansen, Jessie L.
   Ciardi, David R.
   Demory, Brice-Olivier
   Everett, Mark
   Ford, Eric B.
   Haas, Michael R.
   Holman, Matthew J.
   Horch, Elliott
   Jenkins, Jon M.
   Koch, David J.
   Lissauer, Jack J.
   Machalek, Pavel
   Still, Martin
   Welsh, William F.
   Sanderfer, Dwight T.
   Seader, Shawn E.
   Smith, Jeffrey C.
   Thompson, Susan E.
   Twicken, Joseph D.
TI KEPLER-15b: A HOT JUPITER ENRICHED IN HEAVY ELEMENTS AND THE FIRST
   KEPLER MISSION PLANET CONFIRMED WITH THE HOBBY-EBERLY TELESCOPE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planetary systems; stars: individual (Kepler-15, KOI-128, KIC 11359879,
   2MASS J19444814+4908244); techniques: image processing; techniques:
   photometric; techniques: radial velocities; techniques: spectroscopic
ID TRANSITING-PLANET; LIGHT CURVES; SPACED DATA; STARS; SPECTROMETER;
   PERFORMANCE; EVOLUTION; DISCOVERY; PROGRAM; SCIENCE
AB We report the discovery of Kepler-15b (KOI-128), a new transiting exoplanet detected by NASA's Kepler mission. The transit signal with a period of 4.94 days was detected in the quarter 1 (Q1) Kepler photometry. For the first time, we have used the High Resolution Spectrograph (HRS) at the Hobby-Eberly Telescope (HET) to determine the mass of a Kepler planet via precise radial velocity (RV) measurements. The 24 HET/HRS RVs and 6 additional measurements from the Fibre-fed Echelle Spectrograph spectrograph at the Nordic Optical Telescope reveal a Doppler signal with the same period and phase as the transit ephemeris. We used one HET/HRS spectrum of Kepler-15 taken without the iodine cell to determine accurate stellar parameters. The host star is a metal-rich ([Fe/H] = 0.36 +/- 0.07) G-type main-sequence star with T-eff = 5515 +/- 124 K. The semi-amplitude K of the RV orbit is 78.7(-9.5)(+ 8.5) m s(-1), which yields a planet mass of 0.66 +/- 0.1 M-Jup. The planet has a radius of 0.96 +/- 0.06 R-Jup and a mean bulk density of 0.9 +/- 0.2 g cm(-3). The radius of Kepler-15b is smaller than the majority of transiting planets with similar mass and irradiation level. This suggests that the planet is more enriched in heavy elements than most other transiting giant planets. For Kepler-15b we estimate a heavy element mass of 30-40 M-circle plus.
C1 [Endl, Michael; MacQueen, Phillip J.; Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
   [Brugamyer, Erik J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
   [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Denmark Ctr Star & Planet Format, DK-1168 Copenhagen, Denmark.
   [Lucas, Phillip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Demory, Brice-Olivier] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
   [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
   [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
   [Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
   [Jenkins, Jon M.; Sanderfer, Dwight T.; Seader, Shawn E.; Smith, Jeffrey C.; Thompson, Susan E.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Machalek, Pavel] SETI Inst, Mountain View, CA 94043 USA.
   [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Endl, M (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
RI Caldwell, Douglas/L-7911-2014; 
OI Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X;
   Caldwell, Douglas/0000-0003-1963-9616; Fortney,
   Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666;
   Ciardi, David/0000-0002-5741-3047
FU NASA's Science Mission Directorate
FX Funding for this Discovery mission is provided by NASA's Science Mission
   Directorate. We thank the hundreds of people who make this mission
   successful. The Hobby-Eberly Telescope (HET) is a joint project of the
   University of Texas at Austin, the Pennsylvania State University,
   Stanford University, Ludwig-Maximilians-Universitat Munchen, and
   Georg-August-Universitat at Gottingen. The HET is named in honor of its
   principal benefactors, William P. Hobby and Robert E. Eberly. Based in
   part on observations made with the Nordic Optical Telescope, operated on
   the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and
   Sweden, in the Spanish Observatorio del Roque de los Muchachos of the
   Instituto de Astrofisica de Canarias. We also thank the anonymous
   referee for many helpful suggestions to improve the manuscript.
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PT J
AU Ford, EB
   Rowe, JF
   Fabrycky, DC
   Carter, JA
   Holman, MJ
   Lissauer, JJ
   Ragozzine, D
   Steffen, JH
   Batalha, NM
   Borucki, WJ
   Bryson, S
   Caldwell, DA
   Dunham, EW
   Gautier, TN
   Jenkins, JM
   Koch, DG
   Li, J
   Lucas, P
   Marcy, GW
   McCauliff, S
   Mullally, FR
   Quintana, E
   Still, M
   Tenenbaum, P
   Thompson, SE
   Twicken, JD
AF Ford, Eric B.
   Rowe, Jason F.
   Fabrycky, Daniel C.
   Carter, Joshua A.
   Holman, Matthew J.
   Lissauer, Jack J.
   Ragozzine, Darin
   Steffen, Jason H.
   Batalha, Natalie M.
   Borucki, William J.
   Bryson, Steve
   Caldwell, Douglas A.
   Dunham, Edward W.
   Gautier, Thomas N., III
   Jenkins, Jon M.
   Koch, David G.
   Li, Jie
   Lucas, Philip
   Marcy, Geoffrey W.
   McCauliff, Sean
   Mullally, Fergal R.
   Quintana, Elisa
   Still, Martin
   Tenenbaum, Peter
   Thompson, Susan E.
   Twicken, Joseph D.
TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. I. STATISTICAL ANALYSIS OF THE
   FIRST FOUR MONTHS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE methods: statistical; planetary systems; planets and satellites:
   detection; planets and satellites: dynamical evolution and stability;
   techniques: miscellaneous
ID EXTRASOLAR PLANETS; LIGHT CURVES; LOW-MASS; CANDIDATES; SYSTEM;
   DETECTABILITY; EXOMOONS; DENSITY; TRIPLE; STARS
AB The architectures of multiple planet systems can provide valuable constraints on models of planet formation, including orbital migration, and excitation of orbital eccentricities and inclinations. NASA's Kepler mission has identified 1235 transiting planet candidates. The method of transit timing variations (TTVs) has already confirmed seven planets in two planetary systems. We perform a transit timing analysis of the Kepler planet candidates. We find that at least similar to 11% of planet candidates currently suitable for TTV analysis show evidence suggestive of TTVs, representing at least similar to 65 TTV candidates. In all cases, the time span of observations must increase for TTVs to provide strong constraints on planet masses and/or orbits, as expected based on N-body integrations of multiple transiting planet candidate systems (assuming circular and coplanar orbits). We find the fraction of planet candidates showing TTVs in this data set does not vary significantly with the number of transiting planet candidates per star, suggesting significant mutual inclinations and that many stars with a single transiting planet should host additional non-transiting planets. We anticipate that Kepler could confirm (or reject) at least similar to 12 systems with multiple transiting planet candidates via TTVs. Thus, TTVs will provide a powerful tool for confirming transiting planets and characterizing the orbital dynamics of low-mass planets. If Kepler observations were extended to at least seven years, then TTVs would provide much more precise constraints on the dynamics of systems with multiple transiting planets and would become sensitive to planets with orbital periods extending into the habitable zone of solar-type stars.
C1 [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
   [Rowe, Jason F.; Caldwell, Douglas A.; Jenkins, Jon M.; Li, Jie; Mullally, Fergal R.; Quintana, Elisa; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA.
   [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
   [Carter, Joshua A.; Holman, Matthew J.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
   [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
   [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
   [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [McCauliff, Sean] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ford, EB (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
EM eford@astro.ufl.edu
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell,
   Douglas/L-7911-2014; 
OI Caldwell, Douglas/0000-0003-1963-9616; /0000-0001-6545-639X; Fabrycky,
   Daniel/0000-0003-3750-0183
FU National Aeronautics and Space Administration [NNX08AR04G,
   HF-51272.01-A, HF-51267.01-A, NAS 5-26555]; National Science Foundation
   [0707203]; Space Telescope Science Institute
FX Funding for this mission is provided by NASA's Science Mission
   Directorate. We thank the entire Kepler team for the many years of work
   that is proving so successful. We thank David Latham for a careful
   reading of the manuscript. E.B.F. acknowledges support by the National
   Aeronautics and Space Administration under grant NNX08AR04G issued
   through the Kepler Participating Scientist Program. This material is
   based upon work supported by the National Science Foundation under Grant
   No. 0707203. D.C.F. and J.A.C. acknowledge support for this work was
   provided by NASA through Hubble Fellowship grants HF-51272.01-A and
   HF-51267.01-A awarded by the Space Telescope Science Institute, which is
   operated by the Association of Universities for Research in Astronomy,
   Inc., for NASA, under contract NAS 5-26555.
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PT J
AU Fortney, JJ
   Demory, BO
   Desert, JM
   Rowe, J
   Marcy, GW
   Isaacson, H
   Buchhave, LA
   Ciardi, D
   Gautier, TN
   Batalha, NM
   Caldwell, DA
   Bryson, ST
   Nutzman, P
   Jenkins, JM
   Howard, A
   Charbonneau, D
   Knutson, HA
   Howell, SB
   Everett, M
   Fressin, F
   Deming, D
   Borucki, WJ
   Brown, TM
   Ford, EB
   Gilliland, RL
   Latham, DW
   Miller, N
   Seager, S
   Fischer, DA
   Koch, D
   Lissauer, JJ
   Haas, MR
   Still, M
   Lucas, P
   Gillon, M
   Christiansen, JL
   Geary, JC
AF Fortney, Jonathan J.
   Demory, Brice-Olivier
   Desert, Jean-Michel
   Rowe, Jason
   Marcy, Geoffrey W.
   Isaacson, Howard
   Buchhave, Lars A.
   Ciardi, David
   Gautier, Thomas N.
   Batalha, Natalie M.
   Caldwell, Douglas A.
   Bryson, Stephen T.
   Nutzman, Philip
   Jenkins, Jon M.
   Howard, Andrew
   Charbonneau, David
   Knutson, Heather A.
   Howell, Steve B.
   Everett, Mark
   Fressin, Francois
   Deming, Drake
   Borucki, William J.
   Brown, Timothy M.
   Ford, Eric B.
   Gilliland, Ronald L.
   Latham, David W.
   Miller, Neil
   Seager, Sara
   Fischer, Debra A.
   Koch, David
   Lissauer, Jack J.
   Haas, Michael R.
   Still, Martin
   Lucas, Philip
   Gillon, Michael
   Christiansen, Jessie L.
   Geary, John C.
TI DISCOVERY AND ATMOSPHERIC CHARACTERIZATION OF GIANT PLANET KEPLER-12b:
   AN INFLATED RADIUS OUTLIER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planets and satellites: atmospheres; stars: individual (Kepler-12,
   KOI-20, KIC 11804465); techniques: spectroscopic
ID TRANSITING EXTRASOLAR PLANETS; SPITZER-SPACE-TELESCOPE; EXOPLANET HD
   189733B; LIGHT-CURVE PROJECT; B-LIKE PLANETS; HOT JUPITERS; LOW-DENSITY;
   INITIAL CHARACTERISTICS; SECONDARY ECLIPSE; THERMAL STRUCTURE
AB We report the discovery of planet Kepler-12b (KOI-20), which at 1.695 +/- 0.030 R-J is among the handful of planets with super-inflated radii above 1.65 R-J. Orbiting its slightly evolved G0 host with a 4.438 day period, this 0.431 +/- 0.041 M-J planet is the least irradiated within this largest-planet-radius group, which has important implications for planetary physics. The planet's inflated radius and low mass lead to a very low density of 0.111 +/- 0.010 g cm(-3). We detect the occultation of the planet at a significance of 3.7 sigma in the Kepler bandpass. This yields a geometric albedo of 0.14 +/- 0.04; the planetary flux is due to a combination of scattered light and emitted thermal flux. We use multiple observations with Warm Spitzer to detect the occultation at 7 sigma and 4 sigma in the 3.6 and 4.5 mu m bandpasses, respectively. The occultation photometry timing is consistent with a circular orbit at e < 0.01 (1s) and e < 0.09 (3 sigma). The occultation detections across the three bands favor an atmospheric model with no dayside temperature inversion. The Kepler occultation detection provides significant leverage, but conclusions regarding temperature structure are preliminary, given our ignorance of opacity sources at optical wavelengths in hot Jupiter atmospheres. If Kepler-12b and HD 209458b, which intercept similar incident stellar fluxes, have the same heavy-element masses, the interior energy source needed to explain the large radius of Kepler-12b is three times larger than that of HD 209458b. This may suggest that more than one radius-inflation mechanism is at work for Kepler-12b or that it is less heavy-element rich than other transiting planets.
C1 [Fortney, Jonathan J.; Nutzman, Philip; Miller, Neil] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Demory, Brice-Olivier; Seager, Sara] MIT, Cambridge, MA 02139 USA.
   [Desert, Jean-Michel; Buchhave, Lars A.; Charbonneau, David; Fressin, Francois; Latham, David W.; Geary, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Rowe, Jason; Caldwell, Douglas A.; Jenkins, Jon M.; Christiansen, Jessie L.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Marcy, Geoffrey W.; Isaacson, Howard; Howard, Andrew; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
   [Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Gautier, Thomas N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
   [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
   [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
   [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
   [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
   [Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
   [Gillon, Michael] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland.
RP Fortney, JJ (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM jfortney@ucolick.org
RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; 
OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars
   A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Demory,
   Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Fischer,
   Debra/0000-0003-2221-0861; Howard, Andrew/0000-0001-8638-0320; Fortney,
   Jonathan/0000-0002-9843-4354
FU NASA [NNX09AC22G]; NASA's Science Mission Directorate; NASA through
   JPL/Caltech
FX J.J.F. acknowledges the support of the Kepler Participating Scientist's
   program via NASA grant NNX09AC22G. Kepler was competitively selected as
   the tenth Discovery mission. Funding for the Kepler mission is provided
   by NASA's Science Mission Directorate. We thank the many people who gave
   so generously of their time to make the Kepler mission a success. We
   thank Carly Chubak for cross-correlation analyses of the Keck spectra
   for companions. This work incorporates 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. Finally, the authors 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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PT J
AU Fressin, F
   Torres, G
   Desert, JM
   Charbonneau, D
   Batalha, NM
   Fortney, JJ
   Rowe, JF
   Allen, C
   Borucki, WJ
   Brown, TM
   Bryson, ST
   Ciardi, DR
   Cochran, WD
   Deming, D
   Dunham, EW
   Fabrycky, DC
   Gautier, TN
   Gilliland, RL
   Henze, CE
   Holman, MJ
   Howell, SB
   Jenkins, JM
   Kinemuchi, K
   Knutson, H
   Koch, DG
   Latham, DW
   Lissauer, JJ
   Marcy, GW
   Ragozzine, D
   Sasselov, DD
   Still, M
   Tenenbaum, P
   Uddin, K
AF Fressin, Francois
   Torres, Guillermo
   Desert, Jean-Michel
   Charbonneau, David
   Batalha, Natalie M.
   Fortney, Jonathan J.
   Rowe, Jason F.
   Allen, Christopher
   Borucki, William J.
   Brown, Timothy M.
   Bryson, Stephen T.
   Ciardi, David R.
   Cochran, William D.
   Deming, Drake
   Dunham, Edward W.
   Fabrycky, Daniel C.
   Gautier, Thomas N., III
   Gilliland, Ronald L.
   Henze, Christopher E.
   Holman, Matthew J.
   Howell, Steve B.
   Jenkins, Jon M.
   Kinemuchi, Karen
   Knutson, Heather
   Koch, David G.
   Latham, David W.
   Lissauer, Jack J.
   Marcy, Geoffrey W.
   Ragozzine, Darin
   Sasselov, Dimitar D.
   Still, Martin
   Tenenbaum, Peter
   Uddin, Kamal
TI KEPLER-10 c: A 2.2 EARTH RADIUS TRANSITING PLANET IN A MULTIPLE SYSTEM
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: eclipsing; planetary systems; stars: individual (Kepler-10,
   KOI-072, KIC 11904151); stars: statistics
ID SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; LOW-MASS; OBSERVATIONAL
   EVIDENCE; SECONDARY ECLIPSE; BLEND SCENARIOS; LIGHT CURVES; WARM
   SPITZER; CANDIDATES; ATMOSPHERE
AB The Kepler mission has recently announced the discovery of Kepler-10 b, the smallest exoplanet discovered to date and the first rocky planet found by the spacecraft. A second, 45 day period transit-like signal present in the photometry from the first eight months of data could not be confirmed as being caused by a planet at the time of that announcement. Here we apply the light curve modeling technique known as BLENDER to explore the possibility that the signal might be due to an astrophysical false positive (blend). To aid in this analysis we report the observation of two transits with the Spitzer Space Telescope at 4.5 mu m. When combined, they yield a transit depth of 344 +/- 85 ppm that is consistent with the depth in the Kepler passband (376 +/- 9 ppm, ignoring limb darkening), which rules out blends with an eclipsing binary of a significantly different color than the target. Using these observations along with other constraints from high-resolution imaging and spectroscopy, we are able to exclude the vast majority of possible false positives. We assess the likelihood of the remaining blends, and arrive conservatively at a false alarm rate of 1.6 x 10(-5) that is small enough to validate the candidate as a planet (designated Kepler-10 c) with a very high level of confidence. The radius of this object is measured to be R-p = 2.227(-0.057)(+ 0.052) R-circle plus (in which the error includes the uncertainty in the stellar properties), but currently available radial-velocity measurements only place an upper limit on its mass of about 20 M-circle plus. Kepler-10 c represents another example (with Kepler-9 d and Kepler-11 g) of statistical "validation" of a transiting exoplanet, as opposed to the usual "confirmation" that can take place when the Doppler signal is detected or transit timing variations are measured. It is anticipated that many of Kepler's smaller candidates will receive a similar treatment since dynamical confirmation may be difficult or impractical with the sensitivity of current instrumentation.
C1 [Fressin, Francois; Torres, Guillermo; Desert, Jean-Michel; Charbonneau, David; Holman, Matthew J.; Latham, David W.; Ragozzine, Darin; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Batalha, Natalie M.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
   [Fortney, Jonathan J.; Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Allen, Christopher; Tenenbaum, Peter; Uddin, Kamal] Uddin Orbital Sci Corp, Moffett Field, CA 94035 USA.
   [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
   [Ciardi, David R.; Koch, David G.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
   [Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
   [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
   [Jenkins, Jon M.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Kinemuchi, Karen; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
   [Knutson, Heather; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ffressin@cfa.harvard.edu
RI Ragozzine, Darin/C-4926-2013; 
OI Fortney, Jonathan/0000-0002-9843-4354; Ciardi,
   David/0000-0002-5741-3047; Charbonneau, David/0000-0002-9003-484X;
   Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA through JPL/Caltech; NASA
FX Funding for this Discovery mission is provided by NASA's Science Mission
   Directorate. This research has made use of the facilities at the NASA
   Advanced Supercomputing Division (NASA Ames Research Center), and is
   based also 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
   Mukremin Kilic and Rosanne Di Stefano for helpful discussions about
   white dwarfs, and the anonymous referee for constructive comments.
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PT J
AU Gilliland, RL
   Chaplin, WJ
   Dunham, EW
   Argabright, VS
   Borucki, WJ
   Basri, G
   Bryson, ST
   Buzasi, DL
   Caldwell, DA
   Elsworth, YP
   Jenkins, JM
   Koch, DG
   Kolodziejczak, J
   Miglio, A
   Van Cleve, J
   Walkowicz, LM
   Welsh, WF
AF Gilliland, Ronald L.
   Chaplin, William J.
   Dunham, Edward W.
   Argabright, Vic S.
   Borucki, William J.
   Basri, Gibor
   Bryson, Stephen T.
   Buzasi, Derek L.
   Caldwell, Douglas A.
   Elsworth, Yvonne P.
   Jenkins, Jon M.
   Koch, David G.
   Kolodziejczak, Jeffrey
   Miglio, Andrea
   Van Cleve, Jeffrey
   Walkowicz, Lucianne M.
   Welsh, William F.
TI KEPLER MISSION STELLAR AND INSTRUMENT NOISE PROPERTIES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE methods: observational; stars: activity; stars: late-type; stars:
   oscillations; stars: statistics; techniques: photometric
ID MAIN-SEQUENCE STARS; SUN-LIKE STARS; SOLAR-TYPE STARS; RED GIANT STARS;
   CHROMOSPHERIC ACTIVITY; TERRESTRIAL PLANETS; HIERARCHICAL TRIPLE; HYADES
   STARS; MASS STARS; ROTATION
AB Kepler mission results are rapidly contributing to fundamentally new discoveries in both the exoplanet and asteroseismology fields. The data returned from Kepler are unique in terms of the number of stars observed, precision of photometry for time series observations, and the temporal extent of high duty cycle observations. As the first mission to provide extensive time series measurements on thousands of stars over months to years at a level hitherto possible only for the Sun, the results from Kepler will vastly increase our knowledge of stellar variability for quiet solar-type stars. Here, we report on the stellar noise inferred on the timescale of a few hours of most interest for detection of exoplanets via transits. By design the data from moderately bright Kepler stars are expected to have roughly comparable levels of noise intrinsic to the stars and arising from a combination of fundamental limitations such as Poisson statistics and any instrument noise. The noise levels attained by Kepler on-orbit exceed by some 50% the target levels for solar-type, quiet stars. We provide a decomposition of observed noise for an ensemble of 12th magnitude stars arising from fundamental terms (Poisson and readout noise), added noise due to the instrument and that intrinsic to the stars. The largest factor in the modestly higher than anticipated noise follows from intrinsic stellar noise. We show that using stellar parameters from galactic stellar synthesis models, and projections to stellar rotation, activity, and hence noise levels reproduce the primary intrinsic stellar noise features.
C1 [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Chaplin, William J.; Elsworth, Yvonne P.; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
   [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
   [Argabright, Vic S.] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA.
   [Basri, Gibor] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Buzasi, Derek L.] Eureka Sci, Oakland, CA 94602 USA.
   [Caldwell, Douglas A.; Jenkins, Jon M.; Van Cleve, Jeffrey] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Kolodziejczak, Jeffrey] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Gilliland, RL (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM gillil@stsci.edu
RI Caldwell, Douglas/L-7911-2014
OI Caldwell, Douglas/0000-0003-1963-9616
FU NASA's Science Mission Directorate; NASA [NNX09AG09A]; UK Science and
   Technology Facilities Council (STFC)
FX Kepler was competitively selected as the tenth Discovery mission.
   Funding for this mission is provided by NASA's Science Mission
   Directorate. R.L.G. has been partially supported by NASA co-operative
   agreement: NNX09AG09A. W.J.C., Y.E., and A.M. acknowledge support from
   the UK Science and Technology Facilities Council (STFC). A large number
   of people have contributed to make this Mission a success and are
   gratefully thanked for having done so. We thank Jessie Christiansen for
   providing tabulated values of SOC products. Georgi Mandushev and Andrej
   Prsa provided summaries of Besancon model star counts. We thank David
   Soderblom for discussion of expected stellar variability. We thank the
   referee, John Stauffer, for several perceptive remarks and suggestions
   which have served to improve the presentation.
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PT J
AU Lissauer, JJ
   Ragozzine, D
   Fabrycky, DC
   Steffen, JH
   Ford, EB
   Jenkins, JM
   Shporer, A
   Holman, MJ
   Rowe, JF
   Quintana, EV
   Batalha, NM
   Borucki, WJ
   Bryson, ST
   Caldwell, DA
   Carter, JA
   Ciardi, D
   Dunham, EW
   Fortney, JJ
   Gautier, TN
   Howell, SB
   Koch, DG
   Latham, DW
   Marcy, GW
   Morehead, RC
   Sasselov, D
AF Lissauer, Jack J.
   Ragozzine, Darin
   Fabrycky, Daniel C.
   Steffen, Jason H.
   Ford, Eric B.
   Jenkins, Jon M.
   Shporer, Avi
   Holman, Matthew J.
   Rowe, Jason F.
   Quintana, Elisa V.
   Batalha, Natalie M.
   Borucki, William J.
   Bryson, Stephen T.
   Caldwell, Douglas A.
   Carter, Joshua A.
   Ciardi, David
   Dunham, Edward W.
   Fortney, Jonathan J.
   Gautier, Thomas N., III
   Howell, Steve B.
   Koch, David G.
   Latham, David W.
   Marcy, Geoffrey W.
   Morehead, Robert C.
   Sasselov, Dimitar
TI ARCHITECTURE AND DYNAMICS OF KEPLER'S CANDIDATE MULTIPLE TRANSITING
   PLANET SYSTEMS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE celestial mechanics; planets and satellites: dynamical evolution and
   stability; planets and satellites: fundamental parameters; planets and
   satellites: general; planetary systems
ID HOT SUPER-EARTHS; 1ST 4 MONTHS; EXTRASOLAR PLANETS; ORBITAL
   ECCENTRICITIES; SOLAR-SYSTEM; HARPS SEARCH; LIGHT CURVES; SHORT-PERIOD;
   LOW-MASS; RESONANCES
AB About one-third of the similar to 1200 transiting planet candidates detected in the first four months of Kepler data are members of multiple candidate systems. There are 115 target stars with two candidate transiting planets, 45 with three, 8 with four, and 1 each with five and six. We characterize the dynamical properties of these candidate multi-planet systems. The distribution of observed period ratios shows that the vast majority of candidate pairs are neither in nor near low-order mean-motion resonances. Nonetheless, there are small but statistically significant excesses of candidate pairs both in resonance and spaced slightly too far apart to be in resonance, particularly near the 2:1 resonance. We find that virtually all candidate systems are stable, as tested by numerical integrations that assume a nominal mass-radius relationship. Several considerations strongly suggest that the vast majority of these multi-candidate systems are true planetary systems. Using the observed multiplicity frequencies, we find that a single population of planetary systems that matches the higher multiplicities underpredicts the number of singly transiting systems. We provide constraints on the true multiplicity and mutual inclination distribution of the multi-candidate systems, revealing a population of systems with multiple super-Earth-size and Neptune-size planets with low to moderate mutual inclinations.
C1 [Lissauer, Jack J.; Jenkins, Jon M.; Rowe, Jason F.; Quintana, Elisa V.; Caldwell, Douglas A.; Morehead, Robert C.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Ragozzine, Darin; Holman, Matthew J.; Carter, Joshua A.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Fabrycky, Daniel C.; Fortney, Jonathan J.; Latham, David W.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
   [Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
   [Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
   [Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
   [Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
   [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Lissauer, JJ (reprint author), NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Jack.Lissauer@nasa.gov
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell,
   Douglas/L-7911-2014; 
OI Caldwell, Douglas/0000-0003-1963-9616; Fortney,
   Jonathan/0000-0002-9843-4354; Ciardi, David/0000-0002-5741-3047;
   /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [HF-51272.01-A, HF-51267.01-A];
   STScI [NAS 5-26555]
FX Kepler was competitively selected as NASA's tenth Discovery mission.
   Funding for this mission is provided by NASA's Science Mission
   Directorate. The authors thank the many people who gave so generously of
   their time to make the Kepler mission a success. D.C.F. and J.A.C.
   acknowledge NASA support through Hubble Fellowship grants HF-51272.01-A
   and HF-51267.01-A, respectively, awarded by STScI, operated by AURA
   under contract NAS 5-26555. We thank Bill Cochran, Avi Loeb, Hanno Rein,
   Subo Dong, and Bill Welsh for valuable discussions and Kevin Zahnle, Tom
   Greene, Andrew Youdin, and an anonymous reviewer for constructive
   comments on the manuscript. Numerical integrations to test the stability
   of nominal planetary systems were run on the supercomputer Pleiades at
   University of California, Santa Cruz.
NR 83
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2011
VL 197
IS 1
AR 8
DI 10.1088/0067-0049/197/1/8
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400008
ER

PT J
AU Moorhead, AV
   Ford, EB
   Morehead, RC
   Rowe, J
   Borucki, WJ
   Batalha, NM
   Bryson, ST
   Caldwell, DA
   Fabrycky, DC
   Gautier, TN
   Koch, DG
   Holman, MJ
   Jenkins, J
   Li, J
   Lissauer, JJ
   Lucas, P
   Marcy, GW
   Quinn, SN
   Quintana, E
   Ragozzine, D
   Shporer, A
   Still, M
   Torres, G
AF Moorhead, Althea V.
   Ford, Eric B.
   Morehead, Robert C.
   Rowe, Jason
   Borucki, William J.
   Batalha, Natalie M.
   Bryson, Stephen T.
   Caldwell, Douglas A.
   Fabrycky, Daniel C.
   Gautier, Thomas N., III
   Koch, David G.
   Holman, Matthew J.
   Jenkins, Jonm.
   Li, Jie
   Lissauer, Jack J.
   Lucas, Philip
   Marcy, Geoffrey W.
   Quinn, Samuel N.
   Quintana, Elisa
   Ragozzine, Darin
   Shporer, Avi
   Still, Martin
   Torres, Guillermo
TI THE DISTRIBUTION OF TRANSIT DURATIONS FOR KEPLER PLANET CANDIDATES AND
   IMPLICATIONS FOR THEIR ORBITAL ECCENTRICITIES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planets and satellites: fundamental parameters
ID 1ST 4 MONTHS; EXTRASOLAR PLANETS; LIGHT CURVES; TIMING VARIATIONS; HOT
   JUPITERS; SUPER-EARTHS; BINARY; SCATTERING; SYSTEMS; STARS
AB Doppler planet searches have discovered that giant planets follow orbits with a wide range of orbital eccentricities, revolutionizing theories of planet formation. The discovery of hundreds of exoplanet candidates by NASA's Kepler mission enables astronomers to characterize the eccentricity distribution of small exoplanets. Measuring the eccentricity of individual planets is only practical in favorable cases that are amenable to complementary techniques (e.g., radial velocities, transit timing variations, occultation photometry). Yet even in the absence of individual eccentricities, it is possible to study the distribution of eccentricities based on the distribution of transit durations (relative to the maximum transit duration for a circular orbit). We analyze the transit duration distribution of Kepler planet candidates. We find that for host stars with T-eff > 5100K we cannot invert this to infer the eccentricity distribution at this time due to uncertainties and possible systematics in the host star densities. With this limitation in mind, we compare the observed transit duration distribution with models to rule out extreme distributions. If we assume a Rayleigh eccentricity distribution for Kepler planet candidates, then we find best fits with a mean eccentricity of 0.1-0.25 for host stars with T-eff <= 5100 K. We compare the transit duration distribution for different subsets of Kepler planet candidates and discuss tentative trends with planetary radius and multiplicity. High-precision spectroscopic follow-up observations for a large sample of host stars will be required to confirm which trends are real and which are the results of systematic errors in stellar radii. Finally, we identify planet candidates that must be eccentric or have a significantly underestimated stellar radius.
C1 [Moorhead, Althea V.; Ford, Eric B.; Morehead, Robert C.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
   [Rowe, Jason; Caldwell, Douglas A.; Jenkins, Jonm.; Li, Jie; Quintana, Elisa] SETI Inst, Mountain View, CA 94043 USA.
   [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
   [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
   [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Holman, Matthew J.; Quinn, Samuel N.; Ragozzine, Darin; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Marcy, Geoffrey W.; Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Shporer, Avi] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
   [Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Moorhead, AV (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
EM altheam@astro.ufl.edu
RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; 
OI Caldwell, Douglas/0000-0003-1963-9616; /0000-0001-6545-639X; Fabrycky,
   Daniel/0000-0003-3750-0183
FU National Aeronautics and Space Administration [NNX08AR04G]; NASA's
   Science Mission Directorate
FX We thank Bill Cochran, Dave Latham, and Tim Brown for their many helpful
   suggestions and the latter two for their assistance with the Kepler
   Input Catalog, on which this work relies. We thank the entire Kepler
   team for the many years of work that is proving so successful. This
   material is based on work supported by the National Aeronautics and
   Space Administration under grant NNX08AR04G issued through the Kepler
   Participating Scientist Program. Funding for this mission is provided by
   NASA's Science Mission Directorate.
NR 41
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2011
VL 197
IS 1
AR 1
DI 10.1088/0067-0049/197/1/1
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400001
ER

PT J
AU Welsh, WF
   Orosz, JA
   Aerts, C
   Brown, TM
   Brugamyer, E
   Cochran, WD
   Gilliland, RL
   Guzik, JA
   Kurtz, DW
   Latham, DW
   Marcy, GW
   Quinn, SN
   Zima, W
   Allen, C
   Batalha, NM
   Bryson, S
   Buchhave, LA
   Caldwell, DA
   Gautier, TN
   Howell, SB
   Kinemuchi, K
   Ibrahim, KA
   Isaacson, H
   Jenkins, JM
   Prsa, A
   Still, M
   Street, R
   Wohler, B
   Koch, DG
   Borucki, WJ
AF Welsh, William F.
   Orosz, Jerome A.
   Aerts, Conny
   Brown, Timothy M.
   Brugamyer, Erik
   Cochran, William D.
   Gilliland, Ronald L.
   Guzik, Joyce Ann
   Kurtz, D. W.
   Latham, David W.
   Marcy, Geoffrey W.
   Quinn, Samuel N.
   Zima, Wolfgang
   Allen, Christopher
   Batalha, Natalie M.
   Bryson, Steve
   Buchhave, Lars A.
   Caldwell, Douglas A.
   Gautier, Thomas N., III
   Howell, Steve B.
   Kinemuchi, K.
   Ibrahim, Khadeejah A.
   Isaacson, Howard
   Jenkins, Jon M.
   Prsa, Andrej
   Still, Martin
   Street, Rachel
   Wohler, Bill
   Koch, David G.
   Borucki, William J.
TI KOI-54: THE KEPLER DISCOVERY OF TIDALLY EXCITED PULSATIONS AND
   BRIGHTENINGS IN A HIGHLY ECCENTRIC BINARY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: close; binaries: spectroscopic; stars: individual (KID
   8112039, HD 187091, 2MASS J19461553+4356513); stars: oscillations;
   stars: variables: general
ID CLOSE BINARIES; INITIAL CHARACTERISTICS; SPECTROSCOPIC BINARIES; ORBITAL
   PARAMETERS; CADENCE DATA; STELLAR; SYSTEMS; EVOLUTION; OPACITIES;
   SCIENCE
AB Kepler observations of the star HD 187091 (KIC 8112039, hereafter KOI-54) revealed a remarkable light curve exhibiting sharp periodic brightening events every 41.8 days with a superimposed set of oscillations forming a beating pattern in phase with the brightenings. Spectroscopic observations revealed that this is a binary star with a highly eccentric orbit, e = 0.83. We are able to match the Kepler light curve and radial velocities with a nearly face-on (i = 5 degrees.5) binary star model in which the brightening events are caused by tidal distortion and irradiation of nearly identical A stars during their close periastron passage. The two dominant oscillations in the light curve, responsible for the beating pattern, have frequencies that are the 91st and 90th harmonic of the orbital frequency. The power spectrum of the light curve, after removing the binary star brightening component, reveals a large number of pulsations, 30 of which have a signal-to-noise ratio greater than or similar to 7. Nearly all of these pulsations have frequencies that are either integer multiples of the orbital frequency or are tidally split multiples of the orbital frequency. This pattern of frequencies unambiguously establishes the pulsations as resonances between the dynamic tides at periastron and the free oscillation modes of one or both of the stars. KOI-54 is only the fourth star to show such a phenomenon and is by far the richest in terms of excited modes.
C1 [Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
   [Aerts, Conny; Zima, Wolfgang] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
   [Aerts, Conny; Zima, Wolfgang] Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
   [Brown, Timothy M.; Street, Rachel] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
   [Brown, Timothy M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Brugamyer, Erik; Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
   [Brugamyer, Erik; Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
   [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Guzik, Joyce Ann] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
   [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England.
   [Latham, David W.; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Allen, Christopher; Ibrahim, Khadeejah A.; Wohler, Bill] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
   [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
   [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
   [Caldwell, Douglas A.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA.
   [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Kinemuchi, K.; Still, Martin] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
   [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
RP Welsh, WF (reprint author), San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
EM wfw@sciences.sdsu.edu
RI Caldwell, Douglas/L-7911-2014; 
OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars
   A./0000-0003-1605-5666
FU NASA, Science Mission Directorate; NASA [NNX08AR14G]; European Research
   Council under the European Community [227224]; W.M. Keck Foundation
FX Kepler was selected as the 10th mission of the Discovery Program.
   Funding for this mission is provided by NASA, Science Mission
   Directorate. The authors acknowledge support from the Kepler
   Participating Scientists Program via NASA grant NNX08AR14G. C.A. and
   W.Z. received funding from the European Research Council under the
   European Community's Seventh Framework Programme (FP7/2007-2013)/ERC
   grant agreement No. 227224 (PROSPERITY). Some of the data presented
   herein were obtained at the W. M. Keck Observatory, which is operated as
   a scientific partnership among the California Institute of Technology,
   the University of California, and the National Aeronautics and Space
   Administration. The Observatory was made possible by the generous
   financial support of the W. M. Keck Foundation. We thank Gur Windmiller
   for general assistance and for a careful reading of this manuscript. We
   especially thank the many members of the Kepler team whose hard work
   made these observation possible. Finally, we thank the anonymous referee
   for a thorough review of this paper.
NR 38
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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 NOV
PY 2011
VL 197
IS 1
AR 4
DI 10.1088/0067-0049/197/1/4
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400004
ER

PT J
AU Kennedy, K
   Koelbel, C
   Zima, H
AF Kennedy, Ken
   Koelbel, Charles
   Zima, Hans
TI The Rise and Fall of High Performance Fortran
SO COMMUNICATIONS OF THE ACM
LA English
DT Article
ID STANDARD; CHAPEL
C1 [Kennedy, Ken; Koelbel, Charles] Rice Univ, Dept Comp Sci, Houston, TX USA.
   [Zima, Hans] Univ Vienna, A-1010 Vienna, Austria.
   [Koelbel, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM chk@cs.rice.edu; zima@jpl.nasa.gov
NR 22
TC 1
Z9 1
U1 1
U2 4
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 0001-0782
J9 COMMUN ACM
JI Commun. ACM
PD NOV
PY 2011
VL 54
IS 11
BP 74
EP 82
DI 10.1145/2018396.2018415
PG 9
WC Computer Science, Hardware & Architecture; Computer Science, Software
   Engineering; Computer Science, Theory & Methods
SC Computer Science
GA 848LH
UT WOS:000297052600023
ER

PT J
AU Ries, JC
   Ciufolini, I
   Pavlis, EC
   Paolozzi, A
   Koenig, R
   Matzner, RA
   Sindoni, G
   Neumayer, H
AF Ries, J. C.
   Ciufolini, I.
   Pavlis, E. C.
   Paolozzi, A.
   Koenig, R.
   Matzner, R. A.
   Sindoni, G.
   Neumayer, H.
TI The Earth's frame-dragging via laser-ranged satellites: A Response to
   "Some considerations on the present-day results for the detection of
   frame-dragging after the final outcome of GP-B" by Iorio L.
SO EPL
LA English
DT Editorial Material
ID LAGEOS
AB In this letter, we reply to the preceding paper by Iorio (EPL, 96 (2011) 30001 (this issue)), hereafter referred to as I2011, where we address criticisms regarding the Lense-Thirring frame-dragging experiment results obtained from the laser ranging to the two LAGEOS satellites. Copyright (C) EPLA, 2011
C1 [Ries, J. C.] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA.
   [Ciufolini, I.] Univ Salento, Dipartimento Ingn Innovaz, Lecce, Italy.
   [Ciufolini, I.] Ist Nazl Fis Nucl, Sez Lecce, I-73100 Lecce, Italy.
   [Pavlis, E. C.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD USA.
   [Paolozzi, A.; Sindoni, G.] Univ Roma La Sapienza, Scuola Ingn Aerospaziale, Rome, Italy.
   [Koenig, R.; Neumayer, H.] GFZ German Res Ctr Geosci, Potsdam, Germany.
   [Matzner, R. A.] Univ Texas Austin, Ctr Relat, Austin, TX 78712 USA.
RP Ries, JC (reprint author), Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA.
EM ignazio.ciufolini@gmail.com
NR 21
TC 12
Z9 12
U1 0
U2 1
PU EPL ASSOCIATION, EUROPEAN PHYSICAL SOCIETY
PI MULHOUSE
PA 6 RUE DES FRERES LUMIERE, MULHOUSE, 68200, FRANCE
SN 0295-5075
EI 1286-4854
J9 EPL-EUROPHYS LETT
JI EPL
PD NOV
PY 2011
VL 96
IS 3
AR 30002
DI 10.1209/0295-5075/96/30002
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 841UB
UT WOS:000296538200002
ER

PT J
AU Ahn, JH
   Choi, SJ
   Han, JW
   Park, TJ
   Lee, SY
   Choi, YK
AF Ahn, Jae-Hyuk
   Choi, Sung-Jin
   Han, Jin-Woo
   Park, Tae Jung
   Lee, Sang Yup
   Choi, Yang-Kyu
TI Investigation of Size Dependence on Sensitivity for Nanowire FET
   Biosensors
SO IEEE TRANSACTIONS ON NANOTECHNOLOGY
LA English
DT Article
DE Biosensor; capacitive model; double gate (DG); field-effect transistor
   (FET); nanowire (NW)
ID LABEL-FREE DETECTION; ELECTRICAL DETECTION; SILICON NANOWIRES; CARBON
   NANOTUBES; DNA HYBRIDIZATION; NANOSENSORS; DEVICES; SENSORS; MOSFETS;
   SURFACE
AB Label-free electrical detection of biomolecules is demonstrated with a double-gate (DG) nanowire (NW) field-effect transistor (FET). Experimental results confirm that detection sensitivity is favorably improved by the increment of NW size in the DG-NWFET, whereas it is enhanced by the decrement of NW size in a conventional single-gate (SG) NWFET. Sensitivity improvement by the augmentation of the NW size in the DG-FET paves the way to overcome technical challenges we face in achieving ultimate miniaturization of the NW size in the SG-FET. This result is comprehensively understood by simple capacitive modeling. The proposed model explains the observed experimental data and provides a design guideline for highly sensitive NW biosensors.
C1 [Ahn, Jae-Hyuk; Choi, Sung-Jin; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Dept Elect Engn, Taejon 305701, South Korea.
   [Han, Jin-Woo] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
   [Park, Tae Jung; Lee, Sang Yup] Korea Adv Inst Sci & Technol, BioProc Engn Res Ctr, Ctr Syst & Synthet Biotechnol, Inst BioCentury, Taejon 305701, South Korea.
   [Lee, Sang Yup] Korea Adv Inst Sci & Technol, Dept Chem & Biomol Engn, Taejon 305701, South Korea.
   [Lee, Sang Yup] Korea Adv Inst Sci & Technol, Bioinformat Res Ctr, Taejon 305701, South Korea.
   [Lee, Sang Yup] Korea Adv Inst Sci & Technol, Dept Biol Sci, Taejon 305701, South Korea.
   [Lee, Sang Yup] Korea Adv Inst Sci & Technol, Dept Bio & Brain Engn, Taejon 305701, South Korea.
RP Ahn, JH (reprint author), Korea Adv Inst Sci & Technol, Dept Elect Engn, Taejon 305701, South Korea.
EM jhahn@nobelab.kaist.ac.kr; sjchoi@nobelab.kaist.ac.kr;
   jin-woo.han@nasa.gov; tjpark@kaist.ac.kr; leesy@kaist.ac.kr;
   ykchoi@ee.kaist.ac.kr
RI Lee, Sang Yup/C-1526-2011; Park, Tae Jung/G-1509-2013
OI Lee, Sang Yup/0000-0003-0599-3091; 
FU Center for Nanoscale Mechatronics and Manufacturing; Korea Ministry of
   Education, Science and Technology (MEST) [08K1401-00210]; National
   Research and Development Program for the development of biomedical
   function monitoring biosensors [2011-0002182]; National Research
   Foundation of Korea; Korean government [2010-0018931]
FX This work was supported in part by the Center for Nanoscale Mechatronics
   and Manufacturing, one of the 21st Century Frontier Research Programs
   supported by the Korea Ministry of Education, Science and Technology
   (MEST), under Grant 08K1401-00210, in part by the National Research and
   Development Program for the development of biomedical function
   monitoring biosensors under Grant 2011-0002182, and in part by the
   National Research Foundation of Korea funded by the Korean government
   under Grant 2010-0018931. The review of this paper was arranged by
   Associate Editor B. Nelson.
NR 29
TC 10
Z9 10
U1 0
U2 26
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1536-125X
J9 IEEE T NANOTECHNOL
JI IEEE Trans. Nanotechnol.
PD NOV
PY 2011
VL 10
IS 6
BP 1405
EP 1411
DI 10.1109/TNANO.2011.2157519
PG 7
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
   Materials Science, Multidisciplinary; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Materials Science;
   Physics
GA 844JA
UT WOS:000296742300030
ER

PT J
AU Horton, RM
   Gornitz, V
   Bader, DA
   Ruane, AC
   Goldberg, R
   Rosenzweig, C
AF Horton, Radley M.
   Gornitz, Vivien
   Bader, Daniel A.
   Ruane, Alex C.
   Goldberg, Richard
   Rosenzweig, Cynthia
TI Climate Hazard Assessment for Stakeholder Adaptation Planning in New
   York City
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID SEA-LEVEL RISE; CIRCULATION MODEL OUTPUT; OCEAN CIRCULATION; ICE SHEETS;
   SIMULATIONS; UNCERTAINTY; VARIABILITY; PRECIPITATION; 21ST-CENTURY;
   SATELLITE
AB This paper describes a time-sensitive approach to climate change projections that was developed as part of New York City's climate change adaptation process and that has provided decision support to stakeholders from 40 agencies, regional planning associations, and private companies. The approach optimizes production of projections given constraints faced by decision makers as they incorporate climate change into long-term planning and policy. New York City stakeholders, who are well versed in risk management, helped to preselect the climate variables most likely to impact urban infrastructure and requested a projection range rather than a single "most likely" outcome. The climate projections approach is transferable to other regions and is consistent with broader efforts to provide climate services, including impact, vulnerability, and adaptation information. The approach uses 16 GCMs and three emissions scenarios to calculate monthly change factors based on 30-yr average future time slices relative to a 30-yr model baseline. Projecting these model mean changes onto observed station data for New York City yields dramatic changes in the frequency of extreme events such as coastal flooding and dangerous heat events. On the basis of these methods, the current 1-in-10-year coastal flood is projected to occur more than once every 3 years by the end of the century and heat events are projected to approximately triple in frequency. These frequency changes are of sufficient magnitude to merit consideration in long-term adaptation planning, even though the precise changes in extreme-event frequency are highly uncertain.
C1 [Horton, Radley M.; Gornitz, Vivien; Bader, Daniel A.; Ruane, Alex C.; Goldberg, Richard; Rosenzweig, Cynthia] Columbia Univ, Ctr Climate Syst Res, Earth Inst, New York, NY 10025 USA.
   [Horton, Radley M.; Ruane, Alex C.; Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Horton, RM (reprint author), Columbia Univ, Ctr Climate Syst Res, Earth Inst, 2880 Broadway, New York, NY 10025 USA.
EM rh142@columbia.edu
FU Rockefeller Foundation; Office of Science of the U.S. Department of
   Energy
FX This work was supported by the Rockefeller Foundation. We acknowledge
   the modeling groups, the Program for Climate Model Diagnosis and
   Intercomparison (PCMDI) and the WCRP for the CMIP3 multimodel dataset,
   supported by the Office of Science of the U.S. Department of Energy. We
   thank Jonathan Gregory for additional GCM output not available from the
   WCRP dataset. We also thank Adam Freed and Aaron Koch from the Mayor's
   Office of Long Term Planning and Sustainability and Malcolm Bowman from
   the NPCC for comments on prior work that helped to inform this paper. We
   also thank the anonymous reviewers of this manuscript.
NR 95
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U2 55
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD NOV
PY 2011
VL 50
IS 11
BP 2247
EP 2266
DI 10.1175/2011JAMC2521.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 848UK
UT WOS:000297080400005
ER

PT J
AU Wang, CX
   Yang, P
   Baum, BA
   Platnick, S
   Heidinger, AK
   Hu, YX
   Holz, RE
AF Wang, Chenxi
   Yang, Ping
   Baum, Bryan A.
   Platnick, Steven
   Heidinger, Andrew K.
   Hu, Yongxiang
   Holz, Robert E.
TI Retrieval of Ice Cloud Optical Thickness and Effective Particle Size
   Using a Fast Infrared Radiative Transfer Model
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID BULK SCATTERING PROPERTIES; MONTE-CARLO CALCULATIONS; CIRRUS CLOUDS;
   MULTIPLE-SCATTERING; LIGHT-SCATTERING; ABSORPTION PROPERTIES;
   SURFACE-ROUGHNESS; DOUBLING METHOD; CRYSTALS; MODIS
AB A computationally efficient radiative transfer model (RTM) is developed for the inference of ice cloud optical thickness and effective particle size from satellite-based infrared (IR) measurements and is aimed at potential use in operational cloud-property retrievals from multispectral satellite imagery. The RTM employs precomputed lookup tables to simulate the top-of-the-atmosphere (TOA) radiances (or brightness temperatures) at 8.5-, 11-, and 12-mu m bands. For the clear-sky atmosphere, the optical thickness of each atmospheric layer resulting from gaseous absorption is derived from the correlated-k-distribution method. The cloud reflectance, transmittance, emissivity, and effective temperature are precomputed using the Discrete Ordinate Radiative Transfer model (DISORT). For an atmosphere containing a semitransparent ice cloud layer with a visible optical thickness tau smaller than 5, the TOA brightness temperature differences (BTDs) between the fast model and the more rigorous DISORT results are less than 0.1 K, whereas the BTDs are less than 0.01 K if tau is larger than 10. With the proposed RTM, the cloud optical and microphysical properties are retrieved from collocated observations from the Moderate Resolution Imaging Spectroradiometer (MODIS) and Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) in conjunction with the Modern Era Retrospective-Analysis for Research and Applications (MERRA) data. Comparisons between the retrieved ice cloud properties (optical thickness and effective particle size) based on the present IR fast model and those from the Aqua/MODIS operational collection-5 cloud products indicate that the IR retrievals are smaller. A comparison between the IR-retrieved ice water path (IWP) and CALIOP-retrieved IWP shows robust agreement over most of the IWP range.
C1 [Wang, Chenxi; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
   [Baum, Bryan A.; Holz, Robert E.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
   [Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Heidinger, Andrew K.] NOAA, NESDIS Ctr Satellite Applicat & Res, Madison, WI USA.
   [Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM pyang@tamu.edu
RI Yang, Ping/B-4590-2011; Hu, Yongxiang/K-4426-2012; Baum,
   Bryan/B-7670-2011; Platnick, Steven/J-9982-2014; Heidinger,
   Andrew/F-5591-2010
OI Baum, Bryan/0000-0002-7193-2767; Platnick, Steven/0000-0003-3964-3567;
   Heidinger, Andrew/0000-0001-7631-109X
FU NASA [NNX08AP57G, NNX11AF40G]
FX This study was partially supported by NASA Grant NNX08AP57G. Bryan Baum
   and Ping Yang gratefully acknowledge the support provided through NASA
   Grant NNX11AF40G. The views, opinions, and findings contained in this
   report are those of the authors and should not be construed as an
   official National Oceanic and Atmospheric Administration or U.S.
   government position, policy, or decision.
NR 55
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PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD NOV
PY 2011
VL 50
IS 11
BP 2283
EP 2297
DI 10.1175/JAMC-D-11-067.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 848UK
UT WOS:000297080400008
ER

PT J
AU Margutti, R
   Chincarini, G
   Granot, J
   Guidorzi, C
   Berger, E
   Bernardini, MG
   Gehrels, N
   Soderberg, AM
   Stamatikos, M
   Zaninoni, E
AF Margutti, R.
   Chincarini, G.
   Granot, J.
   Guidorzi, C.
   Berger, E.
   Bernardini, M. G.
   Gehrels, N.
   Soderberg, A. M.
   Stamatikos, M.
   Zaninoni, E.
TI X-ray flare candidates in short gamma-ray bursts
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; gamma-ray burst: general
ID LAG-LUMINOSITY RELATION; AFTERGLOW LIGHT CURVES; EXTENDED EMISSION;
   TELESCOPE OBSERVATIONS; TEMPORAL PROPERTIES; PROMPT EMISSION; PEAK
   LUMINOSITY; HOST GALAXIES; NEUTRON-STARS; SWIFT
AB We present the first systematic study of X-ray flare candidates in short gamma-ray bursts (SGRBs) exploiting the large 6-year Swift data base with the aim to constrain the physical nature of such fluctuations. We find that flare candidates appear in different types of SGRB host galaxy environments and show no clear correlation with the X-ray afterglow lifetime; flare candidates are detected both in SGRBs with a bright extended emission in the soft gamma-rays and in SGRBs which do not show such component. We furthermore show that SGRB X-ray flare candidates only partially share the set of observational properties of long GRB (LGRB) flares. In particular, the main parameter driving the duration evolution of X-ray variability episodes in both classes is found to be the elapsed time from the explosion, with very limited dependence on the different progenitors, environments, central engine lifetimes, prompt variability time-scales and energy budgets. On the contrary, SGRB flare candidates significantly differ from LGRB flares in terms of peak luminosity, isotropic energy, flare-to-prompt luminosity ratio and relative variability flux. However, these differences disappear when the central engine time-scales and energy budget are accounted for, suggesting that (i) flare candidates and prompt pulses in SGRBs likely have a common origin; (ii) similar dissipation and/or emission mechanisms are responsible for the prompt and flare emission in LGRBs and SGRBs, with SGRBs being less energetic albeit faster evolving versions of the long class. Finally, we show that in strict analogy to the SGRB prompt emission, flares candidates fall off the lag-luminosity relation defined by LGRBs, thus strengthening the SGRB flare-prompt pulse connection.
C1 [Margutti, R.; Chincarini, G.; Bernardini, M. G.; Zaninoni, E.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
   [Margutti, R.; Berger, E.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Chincarini, G.] Univ Milano Bicocca, Dip Fis G Occhialini, I-20126 Milan, Italy.
   [Granot, J.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
   [Granot, J.] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
   [Granot, J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Guidorzi, C.] Univ Ferrara, Dept Phys, I-44122 Ferarra, Italy.
   [Gehrels, N.; Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
   [Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
   [Zaninoni, E.] Univ Padua, Dip Astron, I-35122 Padua, Italy.
RP Margutti, R (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy.
EM raffaella.margutti@brera.inaf.it
RI Gehrels, Neil/D-2971-2012
FU ASI [SWIFT I/011/07/0]; Ministry of University and Research of Italy
   [PRIN MIUR 2007TNYZXL]; MAE (Ministry of Exterior); University of Milano
   Bicocca, Italy; ERC
FX We thank the anonymous referee for helpful suggestions that improved the
   quality of this work. RM thanks Lorenzo Amati for sharing his data
   before publication. This work is supported by ASI grant SWIFT
   I/011/07/0, by the Ministry of University and Research of Italy (PRIN
   MIUR 2007TNYZXL), by MAE (Ministry of Exterior), by the University of
   Milano Bicocca, Italy and by the ERC advanced research grant 'GRBs'.
NR 77
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 3
BP 2144
EP 2160
DI 10.1111/j.1365-2966.2011.19397.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HX
UT WOS:000297043600035
ER

PT J
AU Symeonidis, M
   Georgakakis, A
   Seymour, N
   Auld, R
   Bock, J
   Brisbin, D
   Buat, V
   Burgarella, D
   Chanial, P
   Clements, DL
   Cooray, A
   Eales, S
   Farrah, D
   Franceschini, A
   Glenn, J
   Griffin, M
   Hatziminaoglou, E
   Ibar, E
   Ivison, RJ
   Mortier, AMJ
   Oliver, SJ
   Page, MJ
   Papageorgiou, A
   Pearson, CP
   Perez-Fournon, I
   Pohlen, M
   Rawlings, JI
   Raymond, G
   Rodighiero, G
   Roseboom, IG
   Rowan-Robinson, M
   Scott, D
   Smith, AJ
   Tugwell, KE
   Vaccari, M
   Vieira, JD
   Vigroux, L
   Wang, L
   Wright, G
AF Symeonidis, M.
   Georgakakis, A.
   Seymour, N.
   Auld, R.
   Bock, J.
   Brisbin, D.
   Buat, V.
   Burgarella, D.
   Chanial, P.
   Clements, D. L.
   Cooray, A.
   Eales, S.
   Farrah, D.
   Franceschini, A.
   Glenn, J.
   Griffin, M.
   Hatziminaoglou, E.
   Ibar, E.
   Ivison, R. J.
   Mortier, A. M. J.
   Oliver, S. J.
   Page, M. J.
   Papageorgiou, A.
   Pearson, C. P.
   Perez-Fournon, I.
   Pohlen, M.
   Rawlings, J. I.
   Raymond, G.
   Rodighiero, G.
   Roseboom, I. G.
   Rowan-Robinson, M.
   Scott, Douglas
   Smith, A. J.
   Tugwell, K. E.
   Vaccari, M.
   Vieira, J. D.
   Vigroux, L.
   Wang, L.
   Wright, G.
TI Herschel/HerMES: the X-ray-infrared correlation for star-forming
   galaxies at z similar to 1
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: general; galaxies: high-redshift; galaxies: starburst;
   infrared: galaxies; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; DEEP-FIELD-NORTH; FORMATION RATE INDICATOR;
   EXTENDED GROTH STRIP; 2-10 KEV LUMINOSITY; STARBURST GALAXIES; FORMATION
   HISTORY; NUMBER COUNTS; OPTICAL-IDENTIFICATION; SPIRAL GALAXIES
AB For the first time, we investigate the X-ray/infrared (IR) correlation for star-forming galaxies (SFGs) at z similar to 1, using SPIRE submm data from the recently launched Herschel Space Observatory and deep X-ray data from the 2-Ms Chandra Deep Field-North survey. We examine the X-ray/IR correlation in the soft X-ray (SX; 0.5-2 keV) and hard X-ray (HX; 2-10 keV) bands by comparing our z similar to 1 SPIRE-detected SFGs to equivalently IR-luminous (L-IR > 10(10) L-circle dot) samples in the local/low-redshift Universe. Our results suggest that the X-ray/IR properties of the SPIRE SFGs are on average similar to those of their local counterparts, as we find no evidence for evolution in the L-SX/L-IR and L-HX/L-IR ratios with redshift. We note, however, that at all redshifts, both L-SX/L-IR and L-HX/L-IR are strongly dependent on IR luminosity, with luminous and ultraluminous IR galaxies (LIRGs and ULIRGs; L-IR > 10(11) L-circle dot) having up to an order of magnitude lower values than normal IR galaxies (L-IR < 10(11) L-circle dot). We derive a L-SX-L-IR relation and confirm the applicability of an existing L-HX-L-IR relation for both local and distant LIRGs and ULIRGs, consistent with a scenario where X-ray luminosity is correlated with the star formation rate.
C1 [Symeonidis, M.; Seymour, N.; Page, M. J.; Rawlings, J. I.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
   [Georgakakis, A.] Natl Observ Athens, Inst Astron, Athens 15236, Greece.
   [Auld, R.; Eales, S.; Griffin, M.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
   [Bock, J.; Cooray, A.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
   [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Brisbin, D.] Cornell Univ, Ithaca, NY 14853 USA.
   [Buat, V.; Burgarella, D.] Univ Aix Marseille, Lab Astrophys Marseille, OAMP, CNRS, F-13388 Marseille 13, France.
   [Chanial, P.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu CNRS, CE Saclay, F-91191 Gif Sur Yvette, France.
   [Clements, D. L.; Mortier, A. M. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
   [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Farrah, D.; Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
   [Franceschini, A.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
   [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
   [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
   [Ibar, E.; Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Pearson, C. P.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
   [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada.
   [Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
   [Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
   [Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
   [Vigroux, L.] UPMC Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France.
RP Symeonidis, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM msy@mssl.ucl.ac.uk
RI Georgakakis, Antonis/K-4457-2013; Ivison, R./G-4450-2011; Vaccari,
   Mattia/R-3431-2016; 
OI Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577;
   Scott, Douglas/0000-0002-6878-9840; Seymour,
   Nicholas/0000-0003-3506-5536
FU CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
   (Spain); SNSB (Sweden); STFC (UK); NASA (USA)
FX MS is grateful for MSSL/UCL support. The team is also extremely grateful
   to Hector Oti-Floranes, Kazushi Iwasawa and Bret Lehmer, for useful
   discussions and for providing us with models and data essential for the
   various comparisons made in this paper. This paper uses data from
   Herschel's submm photometer SPIRE. SPIRE has been developed by a
   consortium of institutes led by Cardiff University (UK) and including
   University of Lethbridge (Canada); NAOC (China); CEA, LAM (France);
   IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory
   (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of
   Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This
   development has been supported by national funding agencies: CSA
   (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
   (Spain); SNSB (Sweden); STFC (UK) and NASA (USA).
NR 111
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PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 3
BP 2239
EP 2252
DI 10.1111/j.1365-2966.2011.19405.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HX
UT WOS:000297043600042
ER

PT J
AU Franks, S
AF Franks, Shannon
TI Enjoy a new perspective of the Earth
SO PHYSICS WORLD
LA English
DT Editorial Material
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Franks, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM shannon.franks@nasa.gov
NR 0
TC 0
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-8585
J9 PHYS WORLD
JI Phys. World
PD NOV
PY 2011
VL 24
IS 11
BP 48
EP 49
PG 2
WC Physics, Multidisciplinary
SC Physics
GA 848TZ
UT WOS:000297079300030
ER

PT J
AU Meszaros, ZS
   Dimmock, JA
   Ploutz-Snyder, R
   Chauhan, SVS
   Abdul-Malak, Y
   Middleton, FA
   Batki, SL
AF Meszaros, Zsuzsa Szombathyne
   Dimmock, Jacqueline A.
   Ploutz-Snyder, Robert
   Chauhan, Sumerendra Vir Singh
   Abdul-Malak, Ynesse
   Middleton, Frank A.
   Batki, Steven L.
TI Accuracy of self-reported medical problems in patients with alcohol
   dependence and co-occurring schizophrenia or schizoaffective disorder
SO SCHIZOPHRENIA RESEARCH
LA English
DT Article
DE Alcohol; Schizophrenia; Schizoaffective disorder; Medical illness;
   Self-report
ID MENTAL-DISORDERS; UNITED-STATES; COMORBIDITY; CARE; MORBIDITY;
   MORTALITY; ILLNESS; PEOPLE; HEALTH; SCALE
AB Background: Schizophrenia and alcohol dependence (AD) are both major risk factors for a variety of medical problems, yet little is known about the medical status of patients in whom both conditions coexist.
   Objective: The objectives of this study are to assess accuracy of self-reported medical problems and to compare the accuracy reports in patients with schizophrenia or schizoaffective disorder and co-occurring AD compared to patients with AD only and to controls. Our hypothesis was that medical problems are under-reported in patients with co-occurring disorders, possibly due to the combination of alcohol use and symptoms of schizophrenia.
   Methods: Self-reported medical diagnoses were recorded and compared to medical records obtained from all area hospitals in 42 patients with schizophrenia and AD, 44 patients with schizoaffective disorder and AD, 41 patients with AD only, and 15 control subjects. Patients underwent medical history, physical examination, and review of medical records. Results: Patients with schizophrenia or schizoaffective disorder and co-occurring AD underreported their medical problems significantly more than patients with AD only and controls. Accuracy of self report was significantly lower in patients with schizophrenia-spectrum disorders plus co-occurring alcohol dependence than in AD alone or in controls. The most commonly underreported diagnoses included coronary artery disease, chronic renal failure, seizure disorder, hyperlipidemia, asthma and hypertension.
   Discussion: In order to detect potentially unreported medical conditions in patients with co-occurring schizophrenia/schizoaffective disorder and alcohol dependence, the use of targeted screening questionnaires is recommended in addition to physical examination and thorough review of medical records. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Meszaros, Zsuzsa Szombathyne; Dimmock, Jacqueline A.; Chauhan, Sumerendra Vir Singh; Abdul-Malak, Ynesse; Batki, Steven L.] SUNY Upstate Med Univ, Dept Psychiat, Syracuse, NY 13210 USA.
   [Ploutz-Snyder, Robert] NASA, Univ Space Res Assoc, Houston, TX USA.
   [Middleton, Frank A.] SUNY Upstate Med Univ, Dept Neurosci Physiol, Syracuse, NY 13210 USA.
   [Batki, Steven L.] UCSF, Dept Psychiat, San Francisco, CA USA.
   [Batki, Steven L.] San Francisco VA Med Ctr, San Francisco, CA USA.
RP Meszaros, ZS (reprint author), SUNY Upstate Med Univ, Dept Psychiat, 750 E Adams St, Syracuse, NY 13210 USA.
EM meszaroz@upstate.edu
FU NIH-NIAAA [RO1 AA01365501, RO1 AA01615103]
FX This research was supported by NIH-NIAAA grant RO1 AA01365501,
   "Naltrexone Treatment of Alcohol Abuse in Schizophrenia" (PI: Batki) and
   by NIH-NIAAA grant RO1 AA01615103 "Peripheral Pathophysiogenomic Markers
   of Ethanol-induced Brain Damage" (PI: Middleton). The NIH had no further
   role in study design; in the collection, analysis and interpretation of
   data; in the writing of the report; and in the decision to submit this
   paper for publication.
NR 32
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0920-9964
EI 1573-2509
J9 SCHIZOPHR RES
JI Schizophr. Res.
PD NOV
PY 2011
VL 132
IS 2-3
BP 190
EP 193
DI 10.1016/j.schres.2011.07.033
PG 4
WC Psychiatry
SC Psychiatry
GA 848ZB
UT WOS:000297092500016
PM 21852074
ER

PT J
AU Beavan, J
   Fielding, E
   Motagh, M
   Samsonov, S
   Donnelly, N
AF Beavan, John
   Fielding, Eric
   Motagh, Mahdi
   Samsonov, Sergey
   Donnelly, Nic
TI Fault Location and Slip Distribution of the 22 February 2011 M-W 6.2
   Christchurch, New Zealand, Earthquake from Geodetic Data
SO SEISMOLOGICAL RESEARCH LETTERS
LA English
DT Article
ID GPS MEASUREMENTS; CANTERBURY; MOTION; PLATE; MODELS; STRAIN; RADAR
C1 [Beavan, John] GNS Sci, Lower Hutt, New Zealand.
   [Fielding, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Motagh, Mahdi] GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, Potsdam, Germany.
   [Motagh, Mahdi] Univ Tehran, Dept Geomat & Surveying Engn, Tehran, Iran.
   [Samsonov, Sergey] European Ctr Geodynam & Seismol, Walferdange, Luxembourg.
   [Donnelly, Nic] Land Informat New Zealand, Wellington, New Zealand.
RP Beavan, J (reprint author), GNS Sci, Lower Hutt, New Zealand.
EM j.beavan@gns.cri.nz
RI Fielding, Eric/A-1288-2007; 
OI Fielding, Eric/0000-0002-6648-8067; Samsonov, Sergey/0000-0002-6798-4847
FU National Aeronautics and Space Administration
FX We thank GeoNet, Trimble Navigation NZ Ltd, Geosystems NZ Ltd, and
   Global Survey Ltd for providing continuous GPS data, and Josh Thomas,
   Dave Collett, Paul Denys, Kirby MacLeod, and Linda Alblas for their
   assistance with the post-earthquake GPS surveys. We thank Stephen
   Bannister and Caroline Holden for providing comments on the manuscript,
   and an anonymous reviewer for a number of suggestions that helped us
   improve the paper. CSK original data is copyright 2011 Italian Space
   Agency; part was provided by e-GEOS, an ASI/Telespazio company, and part
   was provided under CSK AO PI project 2271. ALOS original data is
   copyright 2010 and 2011 METI and JAXA, distributed by GeoGRID and PASCO.
   The inversions used Igor Pro (http://www.wavemetrics.com/); figures were
   prepared using Igor Pro and GMT (http://gmt.soest.hawaii.edu/). Much of
   this research was funded by the New Zealand government. Part of this
   research was performed at the Jet Propulsion Laboratory, California
   Institute of Technology, under contract with the National Aeronautics
   and Space Administration.
NR 27
TC 50
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U1 3
U2 27
PU SEISMOLOGICAL SOC AMER
PI ALBANY
PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA
SN 0895-0695
J9 SEISMOL RES LETT
JI Seismol. Res. Lett.
PD NOV-DEC
PY 2011
VL 82
IS 6
BP 789
EP 799
DI 10.1785/gssrl.82.6.789
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 841VX
UT WOS:000296544400004
ER

PT J
AU Temmer, M
   Veronig, AM
   Gopalswamy, N
   Yashiro, S
AF Temmer, M.
   Veronig, A. M.
   Gopalswamy, N.
   Yashiro, S.
TI Relation Between the 3D-Geometry of the Coronal Wave and Associated CME
   During the 26 April 2008 Event
SO SOLAR PHYSICS
LA English
DT Article
DE Shock waves; Coronal mass ejections
ID EXTREME-ULTRAVIOLET WAVE; MASS EJECTION; EIT WAVES; QUADRATURE
   OBSERVATIONS; SHOCK-WAVES; STEREO; MISSION; HOLE; AIA; SUN
AB We study the kinematical characteristics and 3D geometry of a large-scale coronal wave that occurred in association with the 26 April 2008 flare-CME event. The wave was observed with the EUVI instruments aboard both STEREO spacecraft (STEREO-A and STEREO-B) with a mean speed of similar to aEuro parts per thousand 240 km s(-1). The wave is more pronounced in the eastern propagation direction, and is thus, better observable in STEREO-B images. From STEREO-B observations we derive two separate initiation centers for the wave, and their locations fit with the coronal dimming regions. Assuming a simple geometry of the wave we reconstruct its 3D nature from combined STEREO-A and STEREO-B observations. We find that the wave structure is asymmetric with an inclination toward East. The associated CME has a deprojected speed of similar to aEuro parts per thousand 750 +/- 50 km s(-1), and it shows a non-radial outward motion toward the East with respect to the underlying source region location. Applying the forward fitting model developed by Thernisien, Howard, and Vourlidas (Astrophys. J. 652, 763, 2006), we derive the CME flux rope position on the solar surface to be close to the dimming regions. We conclude that the expanding flanks of the CME most likely drive and shape the coronal wave.
C1 [Temmer, M.; Veronig, A. M.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria.
   [Gopalswamy, N.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Temmer, M (reprint author), Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, Univ Pl 5, A-8010 Graz, Austria.
EM manuela.temmer@uni-graz.at; asv@igam.uni-graz.at;
   nat.gopalswamy@nasa.gov
RI Gopalswamy, Nat/D-3659-2012; Veronig, Astrid/B-8422-2009; 
OI Temmer, Manuela/0000-0003-4867-7558
FU Austrian Science Fund (FWF) [P20867-N16]
FX We thank the referee for helpful comments. M.T. and A.V. gratefully
   acknowledge the Austrian Science Fund (FWF): P20867-N16.
NR 42
TC 16
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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 NOV
PY 2011
VL 273
IS 2
BP 421
EP 432
DI 10.1007/s11207-011-9746-1
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 849LF
UT WOS:000297126300009
ER

PT J
AU Hodis, HN
   Mack, WJ
   Kono, N
   Azen, SP
   Shoupe, D
   Hwang-Levine, J
   Petitti, D
   Whitfield-Maxwell, L
   Yan, MZ
   Franke, AA
   Selzer, RH
AF Hodis, Howard N.
   Mack, Wendy J.
   Kono, Naoko
   Azen, Stanley P.
   Shoupe, Donna
   Hwang-Levine, Juliana
   Petitti, Diana
   Whitfield-Maxwell, Lora
   Yan, Mingzhu
   Franke, Adrian A.
   Selzer, Robert H.
CA Women's Isoflavone Soy Hlth Re
TI Isoflavone Soy Protein Supplementation and Atherosclerosis Progression
   in Healthy Postmenopausal Women A Randomized Controlled Trial
SO STROKE
LA English
DT Article
DE atherosclerosis; cardiovascular disease; intima-media thickness;
   isoflavones; menopause; soy; women
ID ESTROGEN-RECEPTOR-BETA; INTIMA-MEDIA THICKNESS; CORONARY-ARTERY
   ATHEROSCLEROSIS; DIETARY SOY; CYNOMOLGUS MONKEYS; PHYTO-ESTROGENS;
   DEFICIENT MICE; UNITED-STATES; HEART-DISEASE; PHYTOESTROGENS
AB Background and Purpose-Although epidemiological and experimental studies suggest that dietary intake of soy may be cardioprotective, use of isoflavone soy protein (ISP) supplementation as a primary preventive therapy remains unexplored. We determined whether ISP reduces subclinical atherosclerosis assessed as carotid artery intima-media thickness progression.
   Methods-In a double-blind, placebo-controlled trial, 350 postmenopausal women 45 to 92 years of age without diabetes and cardiovascular disease were randomized to 2 evenly divided daily doses of 25 g soy protein containing 91 mg aglycon isoflavone equivalents or placebo for 2.7 years.
   Results-Overall, mean (95% CI) carotid artery intima-media thickness progression rate was 4.77 (3.39-6.16) mu m/year in the ISP group and 5.68 (4.30-7.06) mu m/year in the placebo group. Although carotid artery intima-media thickness progression was reduced on average by 16% in the ISP group relative to the placebo group, this treatment effect was not statistically significant (P=0.36). Among the subgroup of women who were randomized within 5 years of menopause, ISP participants had on average a 68% lower carotid artery intima-media thickness progression rate than placebo participants 2.16 (-1.10 to 5.43) versus 6.79 (3.56-10.01) mu m/year (P=0.05). ISP supplementation had a null effect on women who were >5 years beyond menopause when randomized. There were no major adverse events from ISP supplementation.
   Conclusions-ISP supplementation did not significantly reduce subclinical atherosclerosis progression in postmenopausal women. Subgroup analysis suggests that ISP supplementation may reduce subclinical atherosclerosis in healthy young (median age, 53 years) women at low-risk for cardiovascular disease who were <5 years postmenopausal. These first trial results of their kind warrant further investigation.
C1 [Hodis, Howard N.; Mack, Wendy J.; Kono, Naoko; Azen, Stanley P.; Hwang-Levine, Juliana; Whitfield-Maxwell, Lora; Yan, Mingzhu] Univ So Calif, Keck Sch Med, Atherosclerosis Res Unit, Los Angeles, CA 90033 USA.
   [Hodis, Howard N.; Mack, Wendy J.; Kono, Naoko; Azen, Stanley P.] Univ So Calif, Keck Sch Med, Dept Prevent Med, Los Angeles, CA 90033 USA.
   [Hodis, Howard N.; Whitfield-Maxwell, Lora; Yan, Mingzhu] Univ So Calif, Keck Sch Med, Dept Med, Los Angeles, CA 90033 USA.
   [Shoupe, Donna] Univ So Calif, Keck Sch Med, Dept Obstet & Gynecol, Los Angeles, CA 90033 USA.
   [Hodis, Howard N.; Hwang-Levine, Juliana] Univ So Calif, Sch Pharm, Dept Mol Pharmacol & Toxicol, Los Angeles, CA 90033 USA.
   [Petitti, Diana] Kaiser Permanente So Calif, Dept Res & Evaluat, Pasadena, CA USA.
   [Franke, Adrian A.] Univ Hawaii, Canc Res Ctr Hawaii, Honolulu, HI 96813 USA.
   [Selzer, Robert H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hodis, HN (reprint author), USC Keck Sch Med, Atherosclerosis Res Unit, 2250 Alcazar St,CSC132, Los Angeles, CA 90033 USA.
EM athero@usc.edu
FU National Center for Complementary and Alternative Medicine
   [U01AT-001653]; Office of Research on Women's Health; Office of Dietary
   Supplements;  [P30 CA-71789]
FX This study was supported by National Institutes of Health grant
   U01AT-001653 from the National Center for Complementary and Alternative
   Medicine, the Office of Dietary Supplements, and the Office of Research
   on Women's Health and grant P30 CA-71789. Solae LLC (St Louis, MO)
   provided the study products gratis.
NR 45
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U1 0
U2 7
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0039-2499
J9 STROKE
JI Stroke
PD NOV
PY 2011
VL 42
IS 11
BP 3168
EP U389
DI 10.1161/STROKEAHA.111.620831
PG 12
WC Clinical Neurology; Peripheral Vascular Disease
SC Neurosciences & Neurology; Cardiovascular System & Cardiology
GA 842EM
UT WOS:000296574500266
PM 21903957
ER

PT J
AU Mason, BD
   Hartkopf, WI
   Raghavan, D
   Subasavage, JP
   Roberts, LC
   Turner, NH
   ten Brummelaar, TA
AF Mason, Brian D.
   Hartkopf, William I.
   Raghavan, Deepak
   Subasavage, John P.
   Roberts, Lewis C., Jr.
   Turner, Nils H.
   ten Brummelaar, Theo A.
TI KNOW THE STAR, KNOW THE PLANET. II. SPECKLE INTERFEROMETRY OF EXOPLANET
   HOST STARS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: general; binaries: visual; stars: individual (HD 8673);
   techniques: interferometric
ID SOLAR-TYPE STARS; BINARY STARS; MULTIPLICITY; TELESCOPES
AB A study of the host stars to exoplanets is important for understanding their environment. To that end, we report new speckle observations of a sample of exoplanet host primaries. The bright exoplanet host HD 8673 (= HIP 6702) is revealed to have a companion, although at this time we cannot definitively establish the companion as physical or optical. The observing lists for planet searches and for these observations have for the most part been pre-screened for known duplicity, so the detected binary fraction is lower than what would otherwise be expected. Therefore, a large number of double stars were observed contemporaneously for verification and quality control purposes, to ensure that the lack of detection of companions for exoplanet hosts was valid. In these additional observations, 10 pairs are resolved for the first time and 60 pairs are confirmed. These observations were obtained with the USNO speckle camera on the NOAO 4 m telescopes at both KPNO and CTIO from 2001 to 2010.
C1 [Mason, Brian D.; Hartkopf, William I.] USN Observ, Washington, DC 20392 USA.
   [Raghavan, Deepak] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
   [Subasavage, John P.] Cerro Tololo Interamer Observ, La Serena, Chile.
   [Roberts, Lewis C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Turner, Nils H.; ten Brummelaar, Theo A.] Georgia State Univ, Ctr High Angular Resolut Astron, Mt Wilson, CA 91023 USA.
RP Mason, BD (reprint author), USN Observ, Washington, DC 20392 USA.
EM bdm@usno.navy.mil; wih@usno.navy.mil; raghavan@chara.gsu.edu;
   jsubasavage@ctio.noao.edu; lewis.c.roberts@jpl.nasa.gov;
   nils@chara-array.org; theo@chara-array.org
FU NASA; SIM preparatory science program [NRA98-OSS-007]; Terrestrial
   Planet Finder Foundation [NNH06AF701]
FX The USNO speckle interferometry program has been supported by NASA and
   the SIM preparatory science program through NRA98-OSS-007, SIM Key
   Project MASSIF as well as No. NNH06AF701 issued through the Terrestrial
   Planet Finder Foundation Science program. Thanks are also expressed to
   the U.S. Naval Observatory for their continued support of the Double
   Star Program. A portion of the research in this paper was carried out at
   the Jet Propulsion Laboratory, California Institute of Technology, under
   a contract with the National Aeronautics and Space Administration
   (NASA). This research has made use of the SIMBAD database, operated at
   CDS, Strasbourg, France. Grateful acknowledgment is given to USNO
   interns Dean Kang, Laura Flagg, and Ankit Patel for their processing of
   the speckle pixel data. The telescope operators and observing support
   personnel of KPNO and CTIO continue to provide exceptional support for
   visiting astronomers. Thanks to Alberto Alvarez, Skip Andree, Bill
   Binkert, Gale Brehmer, Bill Gillespie, Angel Guerra, Jim Hutchinson,
   Hillary Mathis, Oscar Saa, Patricio Ugarte, and the rest of the KPNO and
   CTIO staff. We also thank Richard Green of KPNO, who was able to provide
   us with two extra nights on the 4 m Mayall telescope during our 2001
   January run. While we were hampered by poor weather, this additional
   allocation of time certainly helped us achieve a greatly enhanced
   completion fraction. A special thanks is also given to Hal Halbedel, who
   operated the telescope on all or part of each of these new KPNO runs and
   was instrumental in the slit-mask work done at KPNO.
NR 14
TC 10
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2011
VL 142
IS 5
AR 176
DI 10.1088/0004-6256/142/5/176
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000033
ER

PT J
AU Roberts, LC
   Turner, NH
   ten Brummelaar, TA
   Mason, BD
   Hartkopf, WI
AF Roberts, Lewis C., Jr.
   Turner, Nils H.
   ten Brummelaar, Theo A.
   Mason, Brian D.
   Hartkopf, William I.
TI KNOW THE STAR, KNOW THE PLANET. I. ADAPTIVE OPTICS OF EXOPLANET HOST
   STARS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; binaries: close; binaries: visual; instrumentation: adaptive
   optics; planetary systems; techniques: photometric
ID STELLAR COMPANIONS; BINARY STARS; PHOTOMETRY; SYSTEM; CONFIRMATION;
   MULTIPLICITY; ASTROMETRY; SEARCH; RANGE; ORBIT
AB The results of an adaptive optics survey of exoplanet host stars for stellar companions are presented. We used the Advanced Electro-Optical System telescope and its adaptive optics system to collect deep images of the stars in the I band. Sixty-two exoplanet host stars were observed and fifteen multiple star systems were resolved. Of these eight are known multiples, while seven are new candidate binaries. For all binaries, we measured the relative astrometry of the pair and the differential magnitude in the I band. We improved the orbits of HD 19994 and tau Boo. These observations will provide improved statistics on the duplicity of exoplanet host stars and provide an increased understanding of the dynamics of known binary star exoplanet hosts.
C1 [Roberts, Lewis C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Turner, Nils H.; ten Brummelaar, Theo A.] Georgia State Univ, Ctr High Angular Resolut Astron, Mt Wilson, CA 91023 USA.
   [Mason, Brian D.; Hartkopf, William I.] USN Observ, Washington, DC 20392 USA.
RP Roberts, LC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM lewis.c.roberts@jpl.nasa.gov; nils@chara-array.org;
   theo@chara-array.org; bdm@usno.navy.mil; wih@usno.navy.mil
OI Roberts, Lewis/0000-0003-3892-2900
FU AFOSR; NSF [AST 0088498]; AFRL/DE [F29601-00-D-0204]; Jet Propulsion
   Laboratory, California Institute of Technology; National Aeronautics and
   Space Administration; Center for High Angular Resolution Astronomy at
   Georgia State University; Washington Double Star Catalog
FX We thank the numerous staff members of the Maui Space Surveillance
   System who helped make these observations possible. The U.S. Air Force
   provided the telescope time, on-site support, and 80% of the research
   funds for this AFOSR and NSF jointly sponsored research under grant
   number NSF AST 0088498. L.C.R. was funded by AFRL/DE (Contract Number
   F29601-00-D-0204) and by the Jet Propulsion Laboratory, California
   Institute of Technology, under a contract with the National Aeronautics
   and Space Administration. T.A.t.B was supported by the Center for High
   Angular Resolution Astronomy at Georgia State University. This research
   made use of the Washington Double Star Catalog, maintained at the U.S.
   Naval Observatory, the SIMBAD database, operated by the CDS in
   Strasbourg, France, and NASA's Astrophysics Data System. 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.
NR 33
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2011
VL 142
IS 5
AR 175
DI 10.1088/0004-6256/142/5/175
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000032
ER

PT J
AU Slawson, RW
   Prsa, A
   Welsh, WF
   Orosz, JA
   Rucker, M
   Batalha, N
   Doyle, LR
   Engle, SG
   Conroy, K
   Coughlin, J
   Gregg, TA
   Fetherolf, T
   Short, DR
   Windmiller, G
   Fabrycky, DC
   Howell, SB
   Jenkins, J
   Uddin, K
   Mullally, F
   Seader, SE
   Thompson, SE
   Sanderfer, DT
   Borucki, W
   Koch, D
AF Slawson, Robert W.
   Prsa, Andrej
   Welsh, William F.
   Orosz, Jerome A.
   Rucker, Michael
   Batalha, Natalie
   Doyle, Laurance R.
   Engle, Scott G.
   Conroy, Kyle
   Coughlin, Jared
   Gregg, Trevor A.
   Fetherolf, Tara
   Short, Donald R.
   Windmiller, Gur
   Fabrycky, Daniel C.
   Howell, Steve B.
   Jenkins, Jonm.
   Uddin, Kamal
   Mullally, F.
   Seader, Shawn E.
   Thompson, Susan E.
   Sanderfer, Dwight T.
   Borucki, William
   Koch, David
TI KEPLER ECLIPSING BINARY STARS. II. 2165 ECLIPSING BINARIES IN THE SECOND
   DATA RELEASE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; catalogs; stars: fundamental parameters
ID INITIAL CHARACTERISTICS; CADENCE DATA; CM DRACONIS; PLANETS;
   DETECTABILITY; VARIABILITY; PERFORMANCE; SCIENCE; I.
AB The Kepler Mission provides nearly continuous monitoring of similar to 156,000 objects with unprecedented photometric precision. Coincident with the first data release, we presented a catalog of 1879 eclipsing binary systems identified within the 115 deg(2) Kepler field of view (FOV). Here, we provide an updated catalog augmented with the second Kepler data release which increases the baseline nearly fourfold to 125 days. Three hundred and eighty-six new systems have been added, ephemerides and principal parameters have been recomputed. We have removed 42 previously cataloged systems that are now clearly recognized as short-period pulsating variables and another 58 blended systems where we have determined that the Kepler target object is not itself the eclipsing binary. A number of interesting objects are identified. We present several exemplary cases: four eclipsing binaries that exhibit extra (tertiary) eclipse events; and eight systems that show clear eclipse timing variations indicative of the presence of additional bodies bound in the system. We have updated the period and galactic latitude distribution diagrams. With these changes, the total number of identified eclipsing binary systems in the Kepler FOV has increased to 2165, 1.4% of the Kepler target stars. An online version of this catalog is maintained at http://keplerEBs.villanova.edu.
C1 [Slawson, Robert W.; Doyle, Laurance R.] SETI Inst, Mountain View, CA 94043 USA.
   [Prsa, Andrej; Engle, Scott G.; Conroy, Kyle; Coughlin, Jared] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
   [Welsh, William F.; Orosz, Jerome A.; Gregg, Trevor A.; Fetherolf, Tara; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
   [Rucker, Michael; Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
   [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick, Santa Cruz, CA 95064 USA.
   [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
   [Jenkins, Jonm.; Mullally, F.; Seader, Shawn E.; Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
   [Uddin, Kamal] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Slawson, RW (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM rslawson@seti.org; andrej.prsa@villanova.edu
OI Conroy, Kyle/0000-0002-5442-8550; Fabrycky, Daniel/0000-0003-3750-0183
FU NASA/SETI [08-SC-1041]; NSF RUI [AST-05-07542]; NASA [NNX08AR15G,
   NNX08AR14G, NAS5-26555, NNX09AF08G]; National Science Foundation
   [AST-0850564]
FX This work is funded in part by the NASA/SETI subcontract 08-SC-1041 and
   NSF RUI AST-05-07542. Doyle and Slawson are supported by the Kepler
   Mission Participating Scientist Program, NASA grant NNX08AR15G. Welsh
   and Orosz acknowledge support from the Kepler Participating Scientists
   Program via NASA grant NNX08AR14G. We thank the following graduate and
   undergraduate students at San Diego State University who assisted in
   measuring the ephemerides: Gideon Bass, Mallory M. Vale, Michael B.
   Brady, and Camilla Irine Mura (visiting from the Universita degli Studi
   di Pavia, Italy). We gratefully acknowledge the use of computer
   resources made available through Research Experiences for Undergraduates
   (REU) grant AST-0850564 to San Diego State University from the National
   Science Foundation.; 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-Hubble Space Telescope data is provided by the NASA
   Office of Space Science via grant NNX09AF08G and by other grants and
   contracts.
NR 26
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U1 2
U2 10
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 NOV
PY 2011
VL 142
IS 5
AR 160
DI 10.1088/0004-6256/142/5/160
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000017
ER

PT J
AU Stencel, RE
   Kloppenborg, BK
   Wall, RE
   Hopkins, JL
   Howell, SB
   Hoard, DW
   Rayner, J
   Bus, S
   Tokunaga, A
   Sitko, ML
   Bradford, S
   Russell, RW
   Lynch, DK
   Hammel, H
   Whitney, B
   Orton, G
   Yanamandra-Fisher, P
   Hora, JL
   Hinz, P
   Hoffmann, W
   Skemer, A
AF Stencel, Robert E.
   Kloppenborg, Brian K.
   Wall, Randall E., Jr.
   Hopkins, Jeffrey L.
   Howell, Steve B.
   Hoard, D. W.
   Rayner, John
   Bus, Schelte
   Tokunaga, Alan
   Sitko, Michael L.
   Bradford, Suellen
   Russell, Ray W.
   Lynch, David K.
   Hammel, Heidi
   Whitney, Barbara
   Orton, Glenn
   Yanamandra-Fisher, Padma
   Hora, Joseph L.
   Hinz, Philip
   Hoffmann, William
   Skemer, Andrew
TI INFRARED STUDIES OF EPSILON AURIGAE IN ECLIPSE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; protoplanetary disks; stars: individual (epsilon
   Aurigae)
ID SPITZER-SPACE-TELESCOPE; ABSORPTION-LINES; ARRAY CAMERA; SECONDARY;
   SYSTEM; STARS; DISK; SPECTROGRAPH; ULTRAVIOLET; PHOTOMETRY
AB We report here on a series of medium resolution spectro-photometric observations of the enigmatic long period eclipsing binary epsilon Aurigae, during its eclipse interval of 2009-2011, using near-infrared spectra obtained with SpeX on tHe Infrared Telescope Facility (IRTF), mid-infrared spectra obtained with BASS on AOES and IRTF, MIRSI on IRTF, and MIRAC4 on the MMT, along with mid-infrared photometry using MIRSI on IRTF and MIRAC4 on the MMT, plus 1995-2000 timeframe published photometry and data obtained with Denver's TNTCAM2 at WIRO. The goals of these observations included: (1) comparing eclipse depths with prior eclipse data, (2) confirming the re-appearance of CO absorption bands at and after mid-eclipse, associated with sublimation in the disk, (3) seeking evidence for any mid-infrared solid state spectral features from particles in the disk, and (4) providing evidence that the externally irradiated disk has azimuthal temperature differences. IR eclipse depths appear similar to those observed during the most recent (1983) eclipse, although evidence for post-mid-eclipse disk temperature increase is present, due to F star heated portions of the disk coming into view. Molecular CO absorption returned 57 days after nominal mid-eclipse, but was not detected at mid-eclipse plus 34 days, narrowing the association with differentially heated sub-regions in the disk. Transient He I 10830A absorption was detected at mid-eclipse, persisting for at least 90 days thereafter, providing a diagnostic for the hot central region. The lack of solid-state features in Spitzer Infrared Spectrograph, BASS, and MIRAC spectra to date suggests the dominance of large particles (micron-sized) in the disk. Based on these observations, mid-infrared studies out of eclipse can directly monitor and map the disk thermal changes, and better constrain disk opacity and thermal conductivity.
C1 [Stencel, Robert E.; Kloppenborg, Brian K.; Wall, Randall E., Jr.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
   [Hopkins, Jeffrey L.] Hopkins Phoenix Observ, Phoenix, AZ 85033 USA.
   [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
   [Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
   [Rayner, John; Bus, Schelte; Tokunaga, Alan] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
   [Sitko, Michael L.; Bradford, Suellen] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
   [Sitko, Michael L.; Bradford, Suellen; Hammel, Heidi; Whitney, Barbara] Space Sci Inst, Boulder, CO 80301 USA.
   [Russell, Ray W.; Lynch, David K.] Aerosp Corp, Los Angeles, CA 90009 USA.
   [Orton, Glenn; Yanamandra-Fisher, Padma] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Hinz, Philip; Hoffmann, William; Skemer, Andrew] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ 85721 USA.
RP Stencel, RE (reprint author), Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
EM rstencel@du.edu
OI Skemer, Andrew/0000-0001-6098-3924; Hora, Joseph/0000-0002-5599-4650
FU bequest of William Herschel Womble; astronomy at the University of
   Denver; NSF [AST 97-24506, AST 10-16678, JPL RSA 1414715]; NASA ADP
   [NNX09AC73G]; The Aerospace Corporation; National Aeronautics and Space
   Administration, Science Mission Directorate [NNX-08AE38A]
FX This work was supported in part by the bequest of William Herschel
   Womble in support of astronomy at the University of Denver, by NSF
   grants AST 97-24506 and AST 10-16678, and JPL RSA 1414715 to the
   University of Denver, by NASA ADP grant NNX09AC73G to the University of
   Cincinnati, and by The Aerospace Corporation's Independent Research and
   Development Program. Observations reported here were obtained in part as
   Visiting Astronomers at the Infrared Telescope Facility, which is
   operated by the University of Hawaii under Cooperative Agreement
   NNX-08AE38A with the National Aeronautics and Space Administration,
   Science Mission Directorate, Planetary Astronomy Program. Observations
   reported here were obtained in part at the MMT Observatory, a joint
   facility of the Smithsonian Institution and the University of Arizona.
   Observations were also obtained in part at the University of Wyoming's
   Infrared Observatory (WIRO), involving access for which we are grateful.
   The first author thanks Dana Backman for the encouragement to obtain
   mid-IR data during the mid-1990s, and the many observers involved in
   those and all the data reported here. We also thank Jeff Hopkins, Brian
   McCandless, Thomas Rutherford, and the AAVSO for access to their visual
   observation records.
NR 37
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2011
VL 142
IS 5
AR 174
DI 10.1088/0004-6256/142/5/174
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000031
ER

PT J
AU Stritzinger, MD
   Phillips, MM
   Boldt, LN
   Burns, C
   Campillay, A
   Contreras, C
   Gonzalez, S
   Folatelli, G
   Morrell, N
   Krzeminski, W
   Roth, M
   Salgado, F
   DePoy, DL
   Hamuy, M
   Freedman, WL
   Madore, BF
   Marshall, JL
   Persson, SE
   Rheault, JP
   Suntzeff, NB
   Villanueva, S
   Li, WD
   Filippenko, AV
AF Stritzinger, Maximilian D.
   Phillips, M. M.
   Boldt, Luis N.
   Burns, Chris
   Campillay, Abdo
   Contreras, Carlos
   Gonzalez, Sergio
   Folatelli, Gaston
   Morrell, Nidia
   Krzeminski, Wojtek
   Roth, Miguel
   Salgado, Francisco
   DePoy, D. L.
   Hamuy, Mario
   Freedman, Wendy L.
   Madore, Barry F.
   Marshall, J. L.
   Persson, Sven E.
   Rheault, Jean-Philippe
   Suntzeff, Nicholas B.
   Villanueva, Steven
   Li, Weidong
   Filippenko, Alexei V.
TI THE CARNEGIE SUPERNOVA PROJECT: SECOND PHOTOMETRY DATA RELEASE OF
   LOW-REDSHIFT TYPE Ia SUPERNOVAE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: distances and redshifts; supernovae: general
ID STANDARD STARS; ABSOLUTE MAGNITUDES; OPTICAL PHOTOMETRY; LIGHT CURVES;
   WHITE-DWARF; DARK ENERGY; TELESCOPE; SEARCH; SYSTEM; CONSTRAINTS
AB The Carnegie Supernova Project (CSP) was a five-year observational survey conducted at Las Campanas Observatory that obtained, among other things, high-quality light curves of similar to 100 low-redshift Type Ia supernovae (SNe Ia). Presented here is the second data release of nearby SN Ia photometry consisting of 50 objects, with a subset of 45 having near-infrared follow-up observations. Thirty-three objects have optical pre-maximum coverage with a subset of 15 beginning at least five days before maximum light. In the near-infrared, 27 objects have coverage beginning before the epoch of B-band maximum, with a subset of 13 beginning at least five days before maximum. In addition, we present results of a photometric calibration program to measure the CSP optical (uBgVri) bandpasses with an accuracy of similar to 1%. Finally, we report the discovery of a second SN Ia, SN 2006ot, similar in its characteristics to the peculiar SN 2006bt.
C1 [Stritzinger, Maximilian D.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
   [Stritzinger, Maximilian D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
   [Stritzinger, Maximilian D.; Phillips, M. M.; Campillay, Abdo; Morrell, Nidia; Krzeminski, Wojtek; Roth, Miguel] Las Campanas Observ, Carnegie Observ, La Serena, Chile.
   [Boldt, Luis N.] Univ Bonn, Argelander Inst Astron, D-53111 Bonn, Germany.
   [Burns, Chris; Freedman, Wendy L.; Madore, Barry F.; Persson, Sven E.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
   [Contreras, Carlos] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
   [Folatelli, Gaston] Univ Tokyo, IPMU, Chiba 2778583, Japan.
   [Salgado, Francisco] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
   [DePoy, D. L.; Marshall, J. L.; Rheault, Jean-Philippe; Suntzeff, Nicholas B.; Villanueva, Steven] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA.
   [Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile.
   [Madore, Barry F.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Li, Weidong; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Stritzinger, MD (reprint author), Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
EM max.stritzinger@astro.su.se
RI Folatelli, Gaston/A-4484-2011; Hamuy, Mario/G-7541-2016; 
OI stritzinger, maximilian/0000-0002-5571-1833
FU NSF [AST-0306969, AST-0908886, AST-0607438, AST-1008343]; Danish
   National Research Foundation; CONICYT [1060808]; Centro de Astrofisica
   FONDAP [15010003]; Centro BASAL CATA [PFB-06]; Millennium Center for
   Supernova Science [P06-045-F]; TABASGO Foundation; Jet Propulsion
   Laboratory, California Institute of Technology, under the National
   Aeronautics and Space Administration
FX The CSP extends special thanks to the mountain staff of the Las Campanas
   Observatory for their assistance throughout the duration of our
   observational program, and to Jim Hughes for his superb support of our
   network of computers. This material is based upon work supported by the
   NSF under grants AST-0306969, AST-0908886, AST-0607438, and AST-1008343.
   The Dark Cosmology Centre is funded by the Danish National Research
   Foundation. M.H. acknowledges support by CONICYT through grants FONDECYT
   Regular 1060808, Centro de Astrofisica FONDAP 15010003, Centro BASAL
   CATA (PFB-06), and by the Millennium Center for Supernova Science
   (P06-045-F). A.V.F. is grateful for the financial support of the NSF and
   the TABASGO Foundation. 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 49
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2011
VL 142
IS 5
AR 156
DI 10.1088/0004-6256/142/5/156
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000013
ER

PT J
AU Ackermann, M
   Ajello, M
   Allafort, A
   Angelakis, E
   Axelsson, M
   Baldini, L
   Ballet, J
   Barbiellini, G
   Bastieri, D
   Bellazzini, R
   Berenji, B
   Blandford, RD
   Bloom, ED
   Bonamente, E
   Borgland, AW
   Bouvier, A
   Bregeon, J
   Brez, A
   Brigida, M
   Bruel, P
   Buehler, R
   Buson, S
   Caliandro, GA
   Cameron, RA
   Cannon, A
   Caraveo, PA
   Casandjian, JM
   Cavazzuti, E
   Cecchi, C
   Charles, E
   Chekhtman, A
   Cheung, CC
   Ciprini, S
   Claus, R
   Cohen-Tanugi, J
   Cutini, S
   de Palma, F
   Dermer, CD
   Silva, EDE
   Drell, PS
   Dubois, R
   Dumora, D
   Escande, L
   Favuzzi, C
   Fegan, SJ
   Focke, WB
   Fortin, P
   Frailis, M
   Fuhrmann, L
   Fukazawa, Y
   Fusco, P
   Gargano, F
   Gasparrini, D
   Gehrels, N
   Giglietto, N
   Giommi, P
   Giordano, F
   Giroletti, M
   Glanzman, T
   Godfrey, G
   Grandi, P
   Grenier, IA
   Guiriec, S
   Hadasch, D
   Hayashida, M
   Hays, E
   Healey, SE
   Johannesson, G
   Johnson, AS
   Kamae, T
   Katagiri, H
   Kataoka, J
   Knodlseder, J
   Kuss, M
   Lande, J
   Lee, SH
   Longo, F
   Loparco, F
   Lott, B
   Lovellette, MN
   Lubrano, P
   Makeev, A
   Max-Moerbeck, W
   Mazziotta, MN
   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
   Ohsugi, T
   Okumura, A
   Omodei, N
   Orlando, E
   Ormes, JF
   Ozaki, M
   Paneque, D
   Pavlidou, V
   Pelassa, V
   Pepe, M
   Pesce-Rollins, M
   Pierbattista, M
   Piron, F
   Porter, TA
   Raino, S
   Razzano, M
   Readhead, A
   Reimer, A
   Reimer, O
   Richards, JL
   Romani, RW
   Sadrozinski, HFW
   Scargle, JD
   Sgro, C
   Siskind, EJ
   Smith, PD
   Spandre, G
   Spinelli, P
   Strickman, MS
   Suson, DJ
   Takahashi, H
   Tanaka, T
   Taylor, GB
   Thayer, JG
   Thayer, JB
   Thompson, DJ
   Torres, DF
   Tosti, G
   Tramacere, A
   Troja, E
   Vandenbroucke, J
   Vianello, G
   Vitale, V
   Waite, AP
   Wang, P
   Winer, BL
   Wood, KS
   Yang, Z
   Ziegler, M
AF Ackermann, M.
   Ajello, M.
   Allafort, A.
   Angelakis, E.
   Axelsson, M.
   Baldini, L.
   Ballet, J.
   Barbiellini, G.
   Bastieri, D.
   Bellazzini, R.
   Berenji, B.
   Blandford, R. D.
   Bloom, E. D.
   Bonamente, E.
   Borgland, A. W.
   Bouvier, A.
   Bregeon, J.
   Brez, A.
   Brigida, M.
   Bruel, P.
   Buehler, R.
   Buson, S.
   Caliandro, G. A.
   Cameron, R. A.
   Cannon, A.
   Caraveo, P. A.
   Casandjian, J. M.
   Cavazzuti, E.
   Cecchi, C.
   Charles, E.
   Chekhtman, A.
   Cheung, C. C.
   Ciprini, S.
   Claus, R.
   Cohen-Tanugi, J.
   Cutini, S.
   de Palma, F.
   Dermer, C. D.
   do Couto e Silva, E.
   Drell, P. S.
   Dubois, R.
   Dumora, D.
   Escande, L.
   Favuzzi, C.
   Fegan, S. J.
   Focke, W. B.
   Fortin, P.
   Frailis, M.
   Fuhrmann, L.
   Fukazawa, Y.
   Fusco, P.
   Gargano, F.
   Gasparrini, D.
   Gehrels, N.
   Giglietto, N.
   Giommi, P.
   Giordano, F.
   Giroletti, M.
   Glanzman, T.
   Godfrey, G.
   Grandi, P.
   Grenier, I. A.
   Guiriec, S.
   Hadasch, D.
   Hayashida, M.
   Hays, E.
   Healey, S. E.
   Johannesson, G.
   Johnson, A. S.
   Kamae, T.
   Katagiri, H.
   Kataoka, J.
   Knoedlseder, J.
   Kuss, M.
   Lande, J.
   Lee, S. -H.
   Longo, F.
   Loparco, F.
   Lott, B.
   Lovellette, M. N.
   Lubrano, P.
   Makeev, A.
   Max-Moerbeck, W.
   Mazziotta, M. N.
   McEnery, J. E.
   Mehault, J.
   Michelson, P. F.
   Mizuno, T.
   Monte, C.
   Monzani, M. E.
   Morselli, A.
   Moskalenko, I. V.
   Murgia, S.
   Naumann-Godo, M.
   Nishino, S.
   Nolan, P. L.
   Norris, J. P.
   Nuss, E.
   Ohsugi, T.
   Okumura, A.
   Omodei, N.
   Orlando, E.
   Ormes, J. F.
   Ozaki, M.
   Paneque, D.
   Pavlidou, V.
   Pelassa, V.
   Pepe, M.
   Pesce-Rollins, M.
   Pierbattista, M.
   Piron, F.
   Porter, T. A.
   Raino, S.
   Razzano, M.
   Readhead, A.
   Reimer, A.
   Reimer, O.
   Richards, J. L.
   Romani, R. W.
   Sadrozinski, H. F. -W.
   Scargle, J. D.
   Sgro, C.
   Siskind, E. J.
   Smith, P. D.
   Spandre, G.
   Spinelli, P.
   Strickman, M. S.
   Suson, D. J.
   Takahashi, H.
   Tanaka, T.
   Taylor, G. B.
   Thayer, J. G.
   Thayer, J. B.
   Thompson, D. J.
   Torres, D. F.
   Tosti, G.
   Tramacere, A.
   Troja, E.
   Vandenbroucke, J.
   Vianello, G.
   Vitale, V.
   Waite, A. P.
   Wang, P.
   Winer, B. L.
   Wood, K. S.
   Yang, Z.
   Ziegler, M.
TI THE RADIO/GAMMA-RAY CONNECTION IN ACTIVE GALACTIC NUCLEI IN THE ERA OF
   THE FERMI LARGE AREA TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; galaxies: active; galaxies: jets; gamma
   rays: galaxies; radio continuum: galaxies; quasars: general
ID ALL-SKY SURVEY; POLARIMETRY SURVEY; SOURCE CATALOG;
   BACKGROUND-RADIATION; SPECTRUM SOURCES; RADIO-SOURCES; LOUD BLAZARS;
   EMISSION; GALAXIES; AGN
AB We present a detailed statistical analysis of the correlation between radio and gamma-ray emission of the active galactic nuclei (AGNs) detected by Fermi during its first year of operation, with the largest data sets ever used for this purpose. We use both archival interferometric 8.4 GHz data (from the Very Large Array and ATCA, for the full sample of 599 sources) and concurrent single-dish 15 GHz measurements from the Owens Valley Radio Observatory (OVRO, for a sub sample of 199 objects). Our unprecedentedly large sample permits us to assess with high accuracy the statistical significance of the correlation, using a surrogate data method designed to simultaneously account for common-distance bias and the effect of a limited dynamical range in the observed quantities. We find that the statistical significance of a positive correlation between the centimeter radio and the broadband (E > 100 MeV) gamma-ray energy flux is very high for the whole AGN sample, with a probability of < 10(-7) for the correlation appearing by chance. Using the OVRO data, we find that concurrent data improve the significance of the correlation from 1.6 x 10(-6) to 9.0 x 10(-8). Our large sample size allows us to study the dependence of correlation strength and significance on specific source types and gamma-ray energy band. We find that the correlation is very significant (chance probability < 10(-7)) for both flat spectrum radio quasars and BL Lac objects separately; a dependence of the correlation strength on the considered gamma-ray energy band is also present, but additional data will be necessary to constrain its significance.
C1 [Giroletti, M.; Pavlidou, V.; Reimer, A.] INAF Ist Radioastron, I-40129 Bologna, Italy.
   [Ackermann, M.; Ajello, M.; Allafort, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; 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.; Ajello, M.; Allafort, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
   [Angelakis, E.; Fuhrmann, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
   [Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
   [Axelsson, M.] Lund Observ, SE-22100 Lund, Sweden.
   [Axelsson, M.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
   [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
   [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, 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.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
   [Bonamente, E.; Cecchi, C.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
   [Bonamente, E.; Cecchi, C.; Ciprini, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
   [Bouvier, A.; Scargle, J. D.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
   [Bouvier, A.; Sadrozinski, H. F. -W.; Scargle, J. D.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ 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.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
   [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
   [Cannon, A.; Gehrels, N.; Hays, E.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Cannon, A.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
   [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
   [Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy.
   [Chekhtman, A.; Makeev, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
   [Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA.
   [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France.
   [Dermer, C. D.; Lovellette, M. N.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
   [Dumora, D.; Escande, L.; Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
   [Escande, L.] Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France.
   [Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
   [Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
   [Frailis, M.] Osserv Astron Trieste, Ist Nazl Fis Nucl, I-34143 Trieste, Italy.
   [Fukazawa, Y.; Katagiri, H.; Mizuno, T.; Nishino, S.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
   [Grandi, P.] INAF IASF Bologna, I-40129 Bologna, Italy.
   [Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
   [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
   [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
   [Knoedlseder, J.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
   [Max-Moerbeck, W.; Pavlidou, V.; Readhead, A.; Richards, J. L.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [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.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
   [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
   [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
   [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, 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.
   [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
   [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
   [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
   [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
   [Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
   [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
   [Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 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.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
RP Giroletti, M (reprint author), INAF Ist Radioastron, I-40129 Bologna, Italy.
EM afr@slac.stanford.edu; giroletti@ira.inaf.it; pavlidou@astro.caltech.edu
RI Gargano, Fabio/O-8934-2015; Johannesson, Gudlaugur/O-8741-2015;
   Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro,
   Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
   Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery,
   Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano,
   pasquale/F-7269-2012; 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;
   Hays, Elizabeth/D-3257-2012; Pavlidou, Vasiliki/C-2944-2011; Loparco,
   Francesco/O-8847-2015; 
OI Gargano, Fabio/0000-0002-5055-6395; Johannesson,
   Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X;
   Mazziotta, Mario /0000-0001-9325-4672; Torres,
   Diego/0000-0002-1522-9065; Grandi, Paola/0000-0003-1848-6013; giommi,
   paolo/0000-0002-2265-5003; Frailis, Marco/0000-0002-7400-2135; 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;
   Pavlidou, Vasiliki/0000-0002-0870-1368; Loparco,
   Francesco/0000-0002-1173-5673; Tramacere, Andrea/0000-0002-8186-3793;
   Baldini, Luca/0000-0002-9785-7726; SPINELLI, Paolo/0000-0001-6688-8864;
   Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577;
   Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson,
   Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852;
   Angelakis, Emmanouil/0000-0001-7327-5441; Cutini,
   Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X;
   Gasparrini, Dario/0000-0002-5064-9495
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JI Astrophys. J.
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PT J
AU Burgess, JM
   Preece, RD
   Baring, MG
   Briggs, MS
   Connaughton, V
   Guiriec, S
   Paciesas, WS
   Meegan, CA
   Bhat, PN
   Bissaldi, E
   Chaplin, V
   Diehl, R
   Fishman, GJ
   Fitzpatrick, G
   Foley, S
   Gibby, M
   Giles, M
   Goldstein, A
   Greiner, J
   Gruber, D
   van der Horst, AJ
   von Kienlin, A
   Kippen, M
   Kouveliotou, C
   McBreen, S
   Rau, A
   Tierney, D
   Wilson-Hodge, C
AF Burgess, J. Michael
   Preece, Robert D.
   Baring, Matthew G.
   Briggs, Michael S.
   Connaughton, Valerie
   Guiriec, Sylvain
   Paciesas, William S.
   Meegan, Charles A.
   Bhat, P. N.
   Bissaldi, Elisabetta
   Chaplin, Vandiver
   Diehl, Roland
   Fishman, Gerald J.
   Fitzpatrick, Gerard
   Foley, Suzanne
   Gibby, Melissa
   Giles, Misty
   Goldstein, Adam
   Greiner, Jochen
   Gruber, David
   van der Horst, Alexander J.
   von Kienlin, Andreas
   Kippen, Marc
   Kouveliotou, Chryssa
   McBreen, Sheila
   Rau, Arne
   Tierney, Dave
   Wilson-Hodge, Colleen
TI CONSTRAINTS ON THE SYNCHROTRON SHOCK MODEL FOR THE FERMI GRB 090820A
   OBSERVED BY GAMMA-RAY BURST MONITOR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; gamma-ray burst: individual (GRB 090820A);
   gamma rays: stars; methods: data analysis; radiation mechanisms:
   non-thermal; radiation mechanisms: thermal
ID PROMPT EMISSION; SPECTRA; ACCELERATION
AB Discerning the radiative dissipation mechanism for prompt emission in gamma-ray bursts (GRBs) requires detailed spectroscopic modeling that straddles the vF(v) peak in the 100 keV-1 MeV range. Historically, empirical fits such as the popular Band function have been employed with considerable success in interpreting the observations. While extrapolations of the Band parameters can provide some physical insight into the emission mechanisms responsible for GRBs, these inferences do not provide a unique way of discerning between models. By fitting physical models directly, this degeneracy can be broken, eliminating the need for empirical functions; our analysis here offers a first step in this direction. One of the oldest, and leading, theoretical ideas for the production of the prompt signal is the synchrotron shock model. Here we explore the applicability of this model to a bright Fermi gamma-ray burst monitor (GBM) burst with a simple temporal structure, GRB 090820A. Our investigation implements, for the first time, thermal and non-thermal synchrotron emissivities in the RMFIT forward-folding spectral analysis software often used in GBM burst studies. We find that these synchrotron emissivities, together with a blackbody shape, provide at least as good a match to the data as the Band GRB spectral fitting function. This success is achieved in both time-integrated and time-resolved spectral fits.
C1 [Burgess, J. Michael; Preece, Robert D.; Briggs, Michael S.; Connaughton, Valerie; Guiriec, Sylvain; Paciesas, William S.; Bhat, P. N.; Chaplin, Vandiver; Goldstein, Adam] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
   [Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
   [Meegan, Charles A.; van der Horst, Alexander J.] Univ Space Res Assoc, Dept Phys, Huntsville, AL 35899 USA.
   [Bissaldi, Elisabetta; Chaplin, Vandiver; Diehl, Roland; Greiner, Jochen; Gruber, David; von Kienlin, Andreas; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Fishman, Gerald J.; Kouveliotou, Chryssa; Wilson-Hodge, Colleen] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
   [Fitzpatrick, Gerard; Foley, Suzanne; McBreen, Sheila; Tierney, Dave] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
   [Gibby, Melissa; Giles, Misty] Jacobs Technol Inc, Huntsville, AL USA.
   [Kippen, Marc] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Burgess, JM (reprint author), Univ Alabama, Dept Phys, 320 Sparkman Dr, Huntsville, AL 35899 USA.
EM james.m.burgess@nasa.gov; baring@rice.edu
RI Bissaldi, Elisabetta/K-7911-2016; 
OI Burgess, James/0000-0003-3345-9515; McBreen, Sheila/0000-0002-1477-618X;
   Bissaldi, Elisabetta/0000-0001-9935-8106; Preece,
   Robert/0000-0003-1626-7335
FU Alabama Space Grant Consortium through NASA [NNX10AJ80H]; NASA
   [NNX09AT80G, NNH07ZDA001-GLAST]
FX We thank the referee for many useful comments that helped clarify the
   presentation. J.M.B. thankfully acknowledges the support of the Alabama
   Space Grant Consortium through NASA Training Grant NNX10AJ80H. M.G.B. is
   grateful for support under NASA's Fermi Guest Investigator program,
   Cycle 2, through grant NNX09AT80G. A.J.v.d.H. was supported by NASA
   grant NNH07ZDA001-GLAST.
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JI Astrophys. J.
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PT J
AU Chapman, NL
   Goldsmith, PF
   Pineda, JL
   Clemens, DP
   Li, D
   Krco, M
AF Chapman, Nicholas L.
   Goldsmith, Paul F.
   Pineda, Jorge L.
   Clemens, D. P.
   Li, Di
   Krco, Marko
TI THE MAGNETIC FIELD IN TAURUS PROBED BY INFRARED POLARIZATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; polarization
ID STAR-FORMING REGIONS; GIANT MOLECULAR CLOUDS; GAMMA-RAY PULSARS; DARK
   CLOUDS; INTERSTELLAR GRAINS; RADIATIVE TORQUES; VLBA DETERMINATION;
   T-TAURI; POLARIMETRY; DUST
AB We present maps of the plane-of-sky magnetic field within two regions of the Taurus molecular cloud: one in the dense core L1495/B213 filament and the other in a diffuse region to the west. The field is measured from the polarization of background starlight seen through the cloud. In total, we measured 287 high-quality near-infrared polarization vectors in these regions. In L1495/B213, the percent polarization increases with column density up to A(V) similar to 9 mag, the limits of our data. The radiative torques model for grain alignment can explain this behavior, but models that invoke turbulence are inconsistent with the data. We also combine our data with published optical and near-infrared polarization measurements in Taurus. Using this large sample, we estimate the strength of the plane-of-sky component of the magnetic field in nine subregions. This estimation is done with two different techniques that use the observed dispersion in polarization angles. Our values range from 5 to 82 mu G and tend to be higher in denser regions. In all subregions, the critical index of the mass-to-magnetic flux ratio is sub-unity, implying that Taurus is magnetically supported on large scales (similar to 2 pc). Within the region observed, the B213 filament takes a sharp turn to the north and the direction of the magnetic field also takes a sharp turn, switching from being perpendicular to the filament to becoming parallel. This behavior can be understood if we are observing the rim of a bubble. We argue that it has resulted from a supernova remnant associated with a recently discovered nearby gamma-ray pulsar.
C1 [Chapman, Nicholas L.; Goldsmith, Paul F.; Pineda, Jorge L.; Li, Di] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Chapman, Nicholas L.] CIERA, Dept Phys & Astron, Evanston, IL 60208 USA.
   [Clemens, D. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
   [Krco, Marko] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Chapman, NL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 301-429, Pasadena, CA 91109 USA.
EM nchapman@u.northwestern.edu
RI Goldsmith, Paul/H-3159-2016
FU National Aeronautics and Space Administration; NSF [AST-0909030, AST
   06-075500, 09-07790]; NASA; NSF; W.M. Keck Foundation; Boston
   University-Lowell
FX 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. N.L.C.
   acknowledges support from NSF grant AST-0909030 awarded to Northwestern
   University. D.P.C. acknowledges support under NSF AST 06-075500 and
   09-07790.; This research has made use of the SIMBAD database, operated
   at CDS, Strasbourg, France. This research was conducted in part using
   the Mimir instrument, jointly developed at Boston University and Lowell
   Observatory and supported by NASA, NSF, and the W.M. Keck Foundation.;
   Perkins telescope time for this project was awarded under the Boston
   University-Lowell Observatory partnership. Brian Taylor played key roles
   in the smooth operations of both Mimir and the Perkins telescope.
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JI Astrophys. J.
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PT J
AU Dorodnitsyn, A
   Bisnovatyi-Kogan, GS
   Kallman, T
AF Dorodnitsyn, A.
   Bisnovatyi-Kogan, G. S.
   Kallman, T.
TI ACTIVE GALACTIC NUCLEUS OBSCURATION THROUGH DUSTY INFRARED-DOMINATED
   FLOWS. I. RADIATION-HYDRODYNAMICS SOLUTION FOR THE WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; galaxies: active; hydrodynamics; methods:
   numerical
ID FLUX-LIMITED DIFFUSION; X-RAY; TORUS WIND; NGC 1068; DISK; PRESSURE;
   NGC-1068; GALAXY; AGN; UNIFICATION
AB We construct a radiation-hydrodynamics model for the obscuring toroidal structure in active galactic nuclei. In this model the obscuration is produced at parsec scales by a dense, dusty wind which is supported by infrared radiation pressure on dust grains. To find the distribution of radiation pressure, we numerically solve the two-dimensional radiation transfer problem in a flux-limited diffusion approximation. We iteratively couple the solution with calculations of stationary one-dimensional models for the wind and obtain the z-component of the velocity. Our results demonstrate that for active galactic nucleus (AGN) luminosities greater than 0.1 L-edd, external illumination can support a geometrically thick obscuration via outflows driven by infrared radiation pressure. The terminal velocity of marginally Compton-thin models (0.2 < tau(T) < 0.6) is comparable to or greater than the escape velocity. In Compton-thick models the maximum value of the vertical component of the velocity is lower than the escape velocity, suggesting that a significant part of our torus is in the form of failed wind. The results demonstrate that obscuration via normal or failed infrared-driven winds is a viable option for the AGN torus problem and AGN unification models. Such winds can also provide an important channel for AGN feedback.
C1 [Dorodnitsyn, A.; Kallman, T.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
   [Dorodnitsyn, A.] Univ Maryland Baltimore Cty UMBC CRESST, Dept Astron, Baltimore, MD 21250 USA.
   [Bisnovatyi-Kogan, G. S.] Space Res Inst, Moscow, Russia.
RP Dorodnitsyn, A (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
FU NASA Goddard Space Flight Center; NASA [10-ATP10-0171]
FX This research was supported by an appointment at the NASA Goddard Space
   Flight Center, administered by CRESST/UMD through a contract with NASA,
   and by grants from the NASA Astrophysics Theory Program 10-ATP10-0171.
   We also thank the referee for constructive comments, which have led to
   improvement of the manuscript.
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SN 0004-637X
EI 1538-4357
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JI Astrophys. J.
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PT J
AU Fox, OD
   Chevalier, RA
   Skrutskie, MF
   Soderberg, AM
   Filippenko, AV
   Ganeshalingam, M
   Silverman, JM
   Smith, N
   Steele, TN
AF Fox, Ori D.
   Chevalier, Roger A.
   Skrutskie, Michael F.
   Soderberg, Alicia M.
   Filippenko, Alexei V.
   Ganeshalingam, Mohan
   Silverman, Jeffrey M.
   Smith, Nathan
   Steele, Thea N.
TI A SPITZER SURVEY FOR DUST IN TYPE IIn SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; dust, extinction; infrared: stars; stars:
   mass-loss; stars: winds, outflows; supernovae: general
ID CORE-COLLAPSE SUPERNOVAE; LUMINOUS BLUE VARIABLES; WOLF-RAYET STARS;
   MASSIVE STARS; INFRARED ECHO; CIRCUMSTELLAR INTERACTION;
   SPACE-TELESCOPE; SN 2005IP; PRESUPERNOVA EVOLUTION; RADIO-EMISSION
AB Recent observations suggest that Type IIn supernovae (SNe IIn) may exhibit late-time (>100 days) infrared (IR) emission from warm dust more than other types of core-collapse SNe. Mid-IR observations, which span the peak of the thermal spectral energy distribution, provide useful constraints on the properties of the dust and, ultimately, the circumstellar environment, explosion mechanism, and progenitor system. Due to the low SN IIn rate (<10% of all core-collapse SNe), few IR observations exist for this subclass. The handful of isolated studies, however, show late-time IR emission from warm dust that, in some cases, extends for five or six years post-discovery. While previous Spitzer/IRAC surveys have searched for dust in SNe, none have targeted the Type IIn subclass. This paper presents results from a warm Spitzer/IRAC survey of the positions of all 68 known SNe IIn within a distance of 250 Mpc between 1999 and 2008 that have remained unobserved by Spitzer more than 100 days post-discovery. The detection of late-time emission from 10 targets (similar to 15%) nearly doubles the database of existing mid-IR observations of SNe IIn. Although optical spectra show evidence for new dust formation in some cases, the data show that in most cases the likely origin of the mid-IR emission is pre-existing dust, which is continuously heated by optical emission generated by ongoing circumstellar interaction between the forward shock and circumstellar medium. Furthermore, an emerging trend suggests that these SNe decline at similar to 1000-2000 days post-discovery once the forward shock overruns the dust shell. The mass-loss rates associated with these dust shells are consistent with luminous blue variable progenitors.
C1 [Fox, Ori D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Chevalier, Roger A.; Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
   [Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Filippenko, Alexei V.; Ganeshalingam, Mohan; Silverman, Jeffrey M.; Smith, Nathan; Steele, Thea N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Smith, Nathan] Steward Observ, Dept Astron, Tucson, AZ 85721 USA.
RP Fox, OD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ori.d.fox@nasa.gov
FU NASA; NSF [AST-0807727, AST-0908886]; TABASGO Foundation; W. M. Keck
   Foundation; Bill and Marina Kast
FX This work is based on observations made with the Spitzer Space Telescope
   (PID 60122), 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. O.D.F. is grateful for support from the NASA Postdoctoral
   Program (NPP). R.A.C. was supported by NSF grant AST-0807727. A.V.F. is
   grateful for the support of NSF grant AST-0908886 and the TABASGO
   Foundation. J.M.S. thanks Marc J. Staley for a graduate fellowship. Some
   of the data presented herein were obtained at the W. M. Keck
   Observatory, which is operated as a scientific partnership among the
   California Institute of Technology, the University of California, and
   NASA; the observatory was made possible by the generous financial
   support of the W. M. Keck Foundation. The Kast spectrograph on the Lick
   3 m Shane telescope was funded by a gift from Bill and Marina Kast. We
   thank the staffs of the Lick and Keck Observatories for their assistance
   with the observations. We are also grateful to many students and
   postdocs who helped take and reduce the optical spectra.
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PT J
AU Kwon, J
   Tamura, M
   Kandori, R
   Kusakabe, N
   Hashimoto, J
   Nakajima, Y
   Nakamura, F
   Nagayama, T
   Nagata, T
   Hough, JH
   Werner, MW
   Teixeira, PS
AF Kwon, Jungmi
   Tamura, Motohide
   Kandori, Ryo
   Kusakabe, Nobuhiko
   Hashimoto, Jun
   Nakajima, Yasushi
   Nakamura, Fumitaka
   Nagayama, Takahiro
   Nagata, Tetsuya
   Hough, James H.
   Werner, Michael W.
   Teixeira, Paula S.
TI COMPLEX SCATTERED RADIATION FIELDS AND MULTIPLE MAGNETIC FIELDS IN THE
   PROTOSTELLAR CLUSTER IN NGC 2264
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars; ISM: individual objects (NGC
   2264); ISM: structure; polarization; stars: formation
ID YOUNG STELLAR OBJECTS; INFRARED IMAGING POLARIMETRY; INITIAL MASS
   FUNCTION; HERBIG-HARO OBJECTS; STAR-FORMING REGION; BROWN DWARF
   CANDIDATES; MOLECULAR CLOUD CORES; OB1 DARK CLOUD; T-TAURI STARS; PMS
   STARS
AB Near-infrared imaging polarimetry in the J, H, and K-s bands has been carried out for the protostellar cluster region around NGC 2264 IRS 2 in the Monoceros OB1 molecular cloud. Various infrared reflection nebula clusters (IRNCs) associated with NGC 2264 IRS 2 and the IRAS 12 S1 core, as well as local infrared reflection nebulae (IRNe), were detected. The illuminating sources of the IRNe were identified with known or new near-and mid-infrared sources. In addition, 314 point-like sources were detected in all three bands and their aperture polarimetry was studied. Using a color-color diagram, reddened field stars and diskless pre-main-sequence stars were selected to trace the magnetic field (MF) structure of the molecular cloud. The mean polarization position angle of the point-like sources is 81 degrees +/- 29 degrees in the cluster core, and 58 degrees +/- 24 degrees in the perimeter of the cluster core, which is interpreted as the projected direction on the sky of the MF in the observed region of the cloud. The Chandrasekhar-Fermi method gives a rough estimate of the MF strength to be about 100 mu G. A comparison with recent numerical simulations of the cluster formation implies that the cloud dynamics is controlled by the relatively strong MF. The local MF direction is well associated with that of CO outflow for IRAS 12 S1 and consistent with that inferred from submillimeter polarimetry. In contrast, the local MF direction runs roughly perpendicular to the Galactic MF direction.
C1 [Kwon, Jungmi; Tamura, Motohide; Kandori, Ryo; Kusakabe, Nobuhiko; Hashimoto, Jun; Nakajima, Yasushi; Nakamura, Fumitaka] Natl Astron Observ Japan, Tokyo 1818588, Japan.
   [Kwon, Jungmi; Tamura, Motohide] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Tokyo 1818588, Japan.
   [Nagayama, Takahiro] Nagoya Univ, Dept Astrophys, Nagoya, Aichi 4648602, Japan.
   [Nagata, Tetsuya] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
   [Hough, James H.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Werner, Michael W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Teixeira, Paula S.] European So Observ, D-85748 Garching, Germany.
RP Kwon, J (reprint author), Natl Astron Observ Japan, Tokyo 1818588, Japan.
EM jungmi.kwon@nao.ac.jp
RI Teixeira, Paula Stella/O-2289-2013
OI Teixeira, Paula Stella/0000-0002-3665-5784
FU Korean Scholarship Foundation; MEXT [19204018, 22000005]; National
   Aeronautics and Space Administration; National Science Foundation
FX This work was supported by the Korean Scholarship Foundation. M. T. has
   been supported by the MEXT, Grants-in-Aid 19204018 and 22000005. This
   work is based on observations made at the South African Astronomical
   Observatory (Department of Astronomy, Nagoya University). This work is
   based in part on observations made with the Spitzer Space Telescope,
   which is operated by the Jet Propulsion Laboratory, California Institute
   of Technology under a contract with NASA. This publication makes use of
   data products from the Two Micron All Sky Survey, which is a joint
   project of the University of Massachusetts and the Infrared Processing
   and Analysis Center/California Institute of Technology, funded by the
   National Aeronautics and Space Administration and the National Science
   Foundation. This research has made use of the SIMBAD database, operated
   at CDS, Strasbourg, France, as well as IRAF and the IDL Astronomy
   Library.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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PT J
AU Majid, WA
   Naudet, CJ
   Lowe, ST
   Kuiper, TBH
AF Majid, Walid A.
   Naudet, Charles J.
   Lowe, Stephen T.
   Kuiper, Thomas B. H.
TI STATISTICAL STUDIES OF GIANT PULSE EMISSION FROM THE CRAB PULSAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; pulsars: individual (Crab pulsar)
ID RADIO; NEBULA; UNIVERSE
AB We have observed the Crab pulsar with the Deep Space Network Goldstone 70 m antenna at 1664 MHz during three observing epochs for a total of 4 hr. Our data analysis has detected more than 2500 giant pulses, with flux densities ranging from 0.1 kJy to 150 kJy and pulse widths from 125 ns (limited by our bandwidth) to as long as 100 mu s, with median power amplitudes and widths of 1 kJy and 2 mu s, respectively. The most energetic pulses in our sample have energy fluxes of approximately 100 kJy mu s. We have used this large sample to investigate a number of giant pulse emission properties in the Crab pulsar, including correlations among pulse flux density, width, energy flux, phase, and time of arrival. We present a consistent accounting of the probability distributions and threshold cuts in order to reduce pulse-width biases. The excellent sensitivity obtained has allowed us to probe further into the population of giant pulses. We find that a significant portion, no less than 50%, of the overall pulsed energy flux at our observing frequency is emitted in the form of giant pulses.
C1 [Majid, Walid A.; Naudet, Charles J.; Lowe, Stephen T.; Kuiper, Thomas B. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Majid, WA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM walid.a.majid@jpl.nasa.gov
FU Research and Technology Development Grant; U.S. government
FX We thank the staff of DSS-14 who helped in acquiring the data for this
   work. This work was carried out at the the Jet Propulsion Laboratory,
   California Institute of Technology, under a Research and Technology
   Development Grant. U.S. government support acknowledged.
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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
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PT J
AU Muraki, Y
   Han, C
   Bennett, DP
   Suzuki, D
   Monard, LAG
   Street, R
   Jorgensen, UG
   Kundurthy, P
   Skowron, J
   Becker, AC
   Albrow, MD
   Fouque, P
   Heyrovsky, D
   Barry, RK
   Beaulieu, JP
   Wellnitz, DD
   Bond, IA
   Sumi, T
   Dong, S
   Gaudi, BS
   Bramich, M
   Dominik, M
   Abe, F
   Botzler, CS
   Freeman, M
   Fukui, A
   Furusawa, K
   Hayashi, F
   Hearnshaw, JB
   Hosaka, S
   Itow, Y
   Kamiya, K
   Korpela, AV
   Kilmartin, PM
   Lin, W
   Ling, CH
   Makita, S
   Masuda, K
   Matsubara, Y
   Miyake, N
   Nishimoto, K
   Ohnishi, K
   Perrott, YC
   Rattenbury, NJ
   Saito, T
   Skuljan, L
   Sullivan, DJ
   Sweatman, WL
   Tristram, PJ
   Wada, K
   Yock, PCM
   Christie, GW
   DePoy, DL
   Gorbikov, E
   Gould, A
   Kaspi, S
   Lee, CU
   Mallia, F
   Maoz, D
   McCormick, J
   Moorhouse, D
   Natusch, T
   Park, BG
   Pogge, RW
   Polishook, D
   Shporer, A
   Thornley, G
   Yee, JC
   Allan, A
   Browne, P
   Horne, K
   Kains, N
   Snodgrass, C
   Steele, I
   Tsapras, Y
   Batista, V
   Bennett, CS
   Brillant, S
   Caldwell, JAR
   Cassan, A
   Cole, A
   Corrales, R
   Coutures, C
   Dieters, S
   Prester, DD
   Donatowicz, J
   Greenhill, J
   Kubas, D
   Marquette, JB
   Martin, R
   Menzies, J
   Sahu, KC
   Waldman, I
   Williams, A
   Zub, M
   Bourhrous, H
   Matsuoka, Y
   Nagayama, T
   Oi, N
   Randriamanakoto, Z
   Bozza, V
   Burgdorf, MJ
   Novati, SC
   Dreizler, S
   Finet, F
   Glitrup, M
   Harpsoe, K
   Hinse, TC
   Hundertmark, M
   Liebig, C
   Maier, G
   Mancini, L
   Mathiasen, M
   Rahvar, S
   Ricci, D
   Scarpetta, G
   Skottfelt, J
   Surdej, J
   Southworth, J
   Wambsganss, J
   Zimmer, F
   Udalski, A
   Poleski, R
   Wyrzykowski, L
   Ulaczyk, K
   Szymanski, MK
   Kubiak, M
   Pietrzynski, G
   Soszynski, I
AF Muraki, Y.
   Han, C.
   Bennett, D. P.
   Suzuki, D.
   Monard, L. A. G.
   Street, R.
   Jorgensen, U. G.
   Kundurthy, P.
   Skowron, J.
   Becker, A. C.
   Albrow, M. D.
   Fouque, P.
   Heyrovsky, D.
   Barry, R. K.
   Beaulieu, J. -P.
   Wellnitz, D. D.
   Bond, I. A.
   Sumi, T.
   Dong, S.
   Gaudi, B. S.
   Bramich, M.
   Dominik, M.
   Abe, F.
   Botzler, C. S.
   Freeman, M.
   Fukui, A.
   Furusawa, K.
   Hayashi, F.
   Hearnshaw, J. B.
   Hosaka, S.
   Itow, Y.
   Kamiya, K.
   Korpela, A. V.
   Kilmartin, P. M.
   Lin, W.
   Ling, C. H.
   Makita, S.
   Masuda, K.
   Matsubara, Y.
   Miyake, N.
   Nishimoto, K.
   Ohnishi, K.
   Perrott, Y. C.
   Rattenbury, N. J.
   Saito, To.
   Skuljan, L.
   Sullivan, D. J.
   Sweatman, W. L.
   Tristram, P. J.
   Wada, K.
   Yock, P. C. M.
   Christie, G. W.
   DePoy, D. L.
   Gorbikov, E.
   Gould, A.
   Kaspi, S.
   Lee, C. -U.
   Mallia, F.
   Maoz, D.
   McCormick, J.
   Moorhouse, D.
   Natusch, T.
   Park, B. -G.
   Pogge, R. W.
   Polishook, D.
   Shporer, A.
   Thornley, G.
   Yee, J. C.
   Allan, A.
   Browne, P.
   Horne, K.
   Kains, N.
   Snodgrass, C.
   Steele, I.
   Tsapras, Y.
   Batista, V.
   Bennett, C. S.
   Brillant, S.
   Caldwell, J. A. R.
   Cassan, A.
   Cole, A.
   Corrales, R.
   Coutures, Ch
   Dieters, S.
   Prester, D. Dominis
   Donatowicz, J.
   Greenhill, J.
   Kubas, D.
   Marquette, J. -B.
   Martin, R.
   Menzies, J.
   Sahu, K. C.
   Waldman, I.
   Williams, A.
   Zub, M.
   Bourhrous, H.
   Matsuoka, Y.
   Nagayama, T.
   Oi, N.
   Randriamanakoto, Z.
   Bozza, V.
   Burgdorf, M. J.
   Novati, S. Calchi
   Dreizler, S.
   Finet, F.
   Glitrup, M.
   Harpsoe, K.
   Hinse, T. C.
   Hundertmark, M.
   Liebig, C.
   Maier, G.
   Mancini, L.
   Mathiasen, M.
   Rahvar, S.
   Ricci, D.
   Scarpetta, G.
   Skottfelt, J.
   Surdej, J.
   Southworth, J.
   Wambsganss, J.
   Zimmer, F.
   Udalski, A.
   Poleski, R.
   Wyrzykowski, L.
   Ulaczyk, K.
   Szymanski, M. K.
   Kubiak, M.
   Pietrzynski, G.
   Soszynski, I.
CA MOA Collaboration
   FUN Collaboration
   RoboNet Collaboration
   PLANET Collaboration
   IRSF Observers
   MiNDSTEp Consortium
   OGLE Collaboration
TI DISCOVERY AND MASS MEASUREMENTS OF A COLD, 10 EARTH MASS PLANET AND ITS
   HOST STAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro; planetary systems
ID MAGNIFICATION MICROLENSING EVENTS; GRAVITATIONAL LENSING EXPERIMENT;
   STELLAR ATMOSPHERE MODELS; SNOW LINE; EXTRASOLAR PLANETS; GALACTIC
   BULGE; SUPER-EARTHS; JUPITER/SATURN ANALOG; DETERMINISTIC MODEL; CORE
   ACCRETION
AB We present the discovery and mass measurement of the cold, low-mass planet MOA-2009-BLG-266Lb, performed with the gravitational microlensing method. This planet has a mass of m(p) = 10.4 +/- 1.7 M-circle plus and orbits a star of mass M-star = 0.56 +/- 0.09 M-circle dot at a semimajor axis of a = 3.2(-0.5)(+1.9) AU and an orbital period of P = 7.6(-1.5)(+7.7) yrs. The planet and host star mass measurements are enabled by the measurement of the microlensing parallax effect, which is seen primarily in the light curve distortion due to the orbital motion of the Earth. But the analysis also demonstrates the capability to measure the microlensing parallax with the Deep Impact (or EPOXI) spacecraft in a heliocentric orbit. The planet mass and orbital distance are similar to predictions for the critical core mass needed to accrete a substantial gaseous envelope, and thus may indicate that this planet is a "failed" gas giant. This and future microlensing detections will test planet formation theory predictions regarding the prevalence and masses of such planets.
C1 [Han, C.] Chungbuk Natl Univ, Dept Phys, Chonju 371763, South Korea.
   [Muraki, Y.; Wada, K.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan.
   [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
   [Suzuki, D.; Abe, F.; Fukui, A.; Furusawa, K.; Hayashi, F.; Hosaka, S.; Itow, Y.; Kamiya, K.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Nishimoto, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
   [Monard, L. A. G.] Ctr Backyard Astrophys, Bronberg Observ, Pretoria, South Africa.
   [Street, R.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
   [Jorgensen, U. G.; Harpsoe, K.; Hinse, T. C.; Mathiasen, M.; Skottfelt, J.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
   [Jorgensen, U. G.; Harpsoe, K.; Hinse, T. C.; Mathiasen, M.; Skottfelt, J.] Ctr Stars & Planet Format, DK-2100 Copenhagen, Denmark.
   [Kundurthy, P.; Becker, A. C.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
   [Skowron, J.; Gaudi, B. S.; Gould, A.; Pogge, R. W.; Yee, J. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
   [Albrow, M. D.; Hearnshaw, J. B.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
   [Fouque, P.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France.
   [Heyrovsky, D.] Charles Univ Prague, Inst Theoret Phys, CR-18000 Prague, Czech Republic.
   [Barry, R. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Beaulieu, J. -P.; Batista, V.; Cassan, A.; Corrales, R.; Coutures, Ch; Kubas, D.; Marquette, J. -B.] Inst Astrophys, F-75014 Paris, France.
   [Wellnitz, D. D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Bond, I. A.; Lin, W.; Ling, C. H.; Skuljan, L.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, Auckland 1330, New Zealand.
   [Sumi, T.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
   [Dong, S.] Inst Adv Study, Princeton, NJ 08540 USA.
   [Bramich, M.; Kains, N.] European So Observ, D-85748 Garching, Germany.
   [Dominik, M.; Browne, P.; Horne, K.; Liebig, C.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
   [Botzler, C. S.; Freeman, M.; Perrott, Y. C.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand.
   [Korpela, A. V.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
   [Kilmartin, P. M.; Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand.
   [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
   [Rattenbury, N. J.] Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England.
   [Saito, To.; Maoz, D.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
   [Christie, G. W.; Natusch, T.] Auckland Observ, Auckland, New Zealand.
   [DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
   [Gorbikov, E.; Kaspi, S.; Shporer, A.] Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverley Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel.
   [Lee, C. -U.; Park, B. -G.; Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
   [Mallia, F.] Campo Catino Austral Observ, San Pedro De Atacama, Chile.
   [McCormick, J.] Farm Cove Observ, Auckland 1706, New Zealand.
   [Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand.
   [Polishook, D.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
   [Allan, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
   [Snodgrass, C.; Brillant, S.; Kubas, D.] European So Observ, Santiago 19, Chile.
   [Snodgrass, C.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
   [Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
   [Tsapras, Y.] Univ London, Astron Unit, Sch Math Sci, London E1 4NS, England.
   [Bennett, C. S.] MIT, Dept Phys, Cambridge, MA 02139 USA.
   [Caldwell, J. A. R.] McDonald Observ, Ft Davis, TX 79734 USA.
   [Cole, A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
   [Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia.
   [Donatowicz, J.] Vienna Univ Technol, A-1040 Vienna, Austria.
   [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia.
   [Menzies, J.; Randriamanakoto, Z.] S African Astron Observ, ZA-7925 Observatory, South Africa.
   [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Waldman, I.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
   [Zub, M.; Maier, G.; Wambsganss, J.] Univ Heidelberg, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany.
   [Bourhrous, H.] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Cape Town, South Africa.
   [Matsuoka, Y.; Nagayama, T.] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
   [Oi, N.] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
   [Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] Univ Salerno, Dept Phys, I-84084 Fisciano, SA, Italy.
   [Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
   [Burgdorf, M. J.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
   [Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
   [Dreizler, S.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
   [Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
   [Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran 193955531, Iran.
   [Rahvar, S.] IPM, Sch Astron, Tehran 193955531, Iran.
   [Southworth, J.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
   [Udalski, A.; Poleski, R.; Wyrzykowski, L.; Ulaczyk, K.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
   [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile.
   [Glitrup, M.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, 410 Seongbong Rho, Chonju 371763, South Korea.
EM cheongho@chungbuk.ac.kr; bennett@nd.edu
RI Wellnitz, Dennis/B-4080-2012; Gaudi, Bernard/I-7732-2012; Dong,
   Subo/J-7319-2012; Greenhill, John/C-8367-2013; Williams,
   Andrew/K-2931-2013; Zimmer, Fabian/M-4765-2014; Skowron,
   Jan/M-5186-2014; Heyrovsky, David/A-2031-2015; Rahvar,
   Sohrab/A-9350-2008; Hundertmark, Markus/C-6190-2015; 
OI Cole, Andrew/0000-0003-0303-3855; Ricci, Davide/0000-0002-9790-0552;
   Snodgrass, Colin/0000-0001-9328-2905; Williams,
   Andrew/0000-0001-9080-0105; Skowron, Jan/0000-0002-2335-1730; Heyrovsky,
   David/0000-0002-5198-5343; Rahvar, Sohrab/0000-0002-7084-5725;
   Hundertmark, Markus/0000-0003-0961-5231; Dominik,
   Martin/0000-0002-3202-0343
FU National Research Foundation of Korea [2009-0081561]; Czech Science
   Foundation [GACR P209/10/1318]; NSF [AST-0757888]; European Research
   Council [246678]; ESO [385.C-0797]; NASA [NNX06Af40G]; Communaute
   francaise de Belgique-Actions de recherche concertees-Academie
   universitaire Wallonie-Europe;  [NASA-NNX10AI81G];  [NSFAST-0708890]; 
   [AST-1009621];  [JSPS18253002];  [JSPS20340052]
FX We acknowledge the following support: NASA-NNX10AI81G, NSFAST-0708890,
   and AST-1009621 (D. P. B.); National Research Foundation of Korea
   2009-0081561 (C.H.); JSPS18253002 and JSPS20340052 (F.A.); Czech Science
   Foundation grant GACR P209/10/1318 (D.H.); NSF Graduate Research
   Fellowship (J.C.Y.); European Research Council Advanced Grant No. 246678
   (A.U.); ESO Prog.ID 385.C-0797( A); NASA NNX06Af40G (B.S.G., A.G.,
   R.W.P.); NSF AST-0757888 (A.G.). D.R. (boursier FRIA), F.F., and J.S.
   acknowledge support from the Communaute francaise de Belgique-Actions de
   recherche concertees-Academie universitaire Wallonie-Europe.
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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
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PT J
AU Robinson, TD
AF Robinson, Tyler D.
TI MODELING THE INFRARED SPECTRUM OF THE EARTH-MOON SYSTEM: IMPLICATIONS
   FOR THE DETECTION AND CHARACTERIZATION OF EARTHLIKE EXTRASOLAR PLANETS
   AND THEIR MOONLIKE COMPANIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; Earth; infrared: planetary systems; Moon; planets and
   satellites: detection; techniques: miscellaneous
ID AURA SATELLITE; LIGHT CURVES; SURFACE; OBLIQUITY; MISSION; OCEANS; DISK
AB The Moon maintains large surface temperatures on its illuminated hemisphere and can contribute significant amounts of flux to spatially unresolved thermal infrared (IR) observations of the Earth-Moon system, especially at wavelengths where Earth's atmosphere is absorbing. In this paper we investigate the effects of an unresolved companion on IR observations of Earthlike exoplanets. For an extrasolar twin Earth-Moon system observed at full phase at IR wavelengths, the Moon consistently comprises about 20% of the total signal, approaches 30% of the signal in the 9.6 mu m ozone band and the 15 mu m carbon dioxide band, makes up as much as 80% of the signal in the 6.3 mu m water band, and more than 90% of the signal in the 4.3 mu m carbon dioxide band. These excesses translate to inferred brightness temperatures for Earth that are too large by 20-40 K and demonstrate that the presence of undetected satellites can have significant impacts on the spectroscopic characterization of exoplanets. The thermal flux contribution from an airless companion depends strongly on phase, implying that observations of exoplanets should be taken when the star-planet-observer angle (i.e., phase angle) is as large as feasibly possible if contributions from companions are to be minimized. We show that, by differencing IR observations of an Earth twin with a companion taken at both gibbous and crescent phases, Moonlike satellites may be detectable by future exoplanet characterization missions for a wide range of system inclinations.
C1 [Robinson, Tyler D.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RP Robinson, TD (reprint author), NASA, Astrobiol Inst, Washington, DC 20546 USA.
EM robinson@astro.washington.edu
FU National Aeronautics and Space Administration through the NASA
   Astrobiology Institute [NNH05ZDA001C]
FX This work was performed as part of the NASA Astrobiology Institute's
   Virtual Planetary Laboratory, supported by the National Aeronautics and
   Space Administration through the NASA Astrobiology Institute under
   solicitation No. NNH05ZDA001C. I thank Vikki Meadows, Eric Agol, David
   Crisp, and Josh Bandfield for discussions and insights provided
   throughout the course of this project. Some of the results in this paper
   have been derived using the HEALPix (Gorski et al. 2005) package.
NR 45
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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 1
PY 2011
VL 741
IS 1
AR 51
DI 10.1088/0004-637X/741/1/51
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000051
ER

PT J
AU Rowe, B
   Hirata, C
   Rhodes, J
AF Rowe, Barnaby
   Hirata, Christopher
   Rhodes, Jason
TI OPTIMAL LINEAR IMAGE COMBINATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark energy; gravitational lensing: weak; methods: data analysis;
   techniques: image processing; techniques: photometric
ID GALAXY SHAPE MEASUREMENT; WEAK LENSING SURVEYS; SHEAR; DETECTORS
AB A simple, yet general, formalism for the optimized linear combination of astrophysical images is constructed and demonstrated. The formalism allows the user to combine multiple undersampled images to provide oversampled output at high precision. The proposed method is general and may be used for any configuration of input pixels and point spread function; it also provides the noise covariance in the output image along with a powerful metric for describing undesired distortion to the image convolution kernel. The method explicitly provides knowledge and control of the inevitable compromise between noise and fidelity in the output image. We present a first prototype implementation of the method, outlining the steps taken to generate an efficient algorithm. This implementation is then put to practical use in reconstructing fully sampled output images using simulated, undersampled input exposures that are designed to mimic the proposed Wide-field InfraRed Survey Telescope (WFIRST). We examine results using randomly rotated and dithered input images, while also assessing better-known "ideal" dither patterns: comparing results, we illustrate the use of the method as a survey design tool. Finally, we use the method to test the robustness of linear image combination when subjected to practical realities such as missing input pixels and focal plane plate scale variations.
C1 [Rowe, Barnaby; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Hirata, Christopher] CALTECH, Dept Astrophys, Pasadena, CA 91106 USA.
RP Rowe, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM browe@caltech.edu; chirata@tapir.caltech.edu;
   jason.d.rhodes@jpl.nasa.gov
OI Rowe, Barnaby/0000-0002-7042-9174
FU National Aeronautics and Space Administration (NASA); NASA WFIRST
   Project Office; Department of Energy [DE- FG03-02-ER40701]; National
   Science Foundation [AST-0807337]; David & Lucile Packard Foundation
FX The authors thank Tod Lauer and Gary Bernstein (particularly regarding
   the use of lookup tables for calculating the system matrices A<INF>alpha
   ij</INF> and B<INF>alpha i</INF>) for useful discussion and suggestions,
   and the anonymous referee for useful comments that improved the
   manuscript. This work was performed in part at the Jet Propulsion
   Laboratory, operated by the California Institute of Technology under a
   contract for the National Aeronautics and Space Administration (NASA).
   B. R. is supported by the NASA WFIRST Project Office. C. H. is supported
   by the Department of Energy (DE- FG03-02-ER40701), the National Science
   Foundation (AST-0807337), and the David & Lucile Packard Foundation.
NR 36
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2011
VL 741
IS 1
AR 46
DI 10.1088/0004-637X/741/1/46
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000046
ER

PT J
AU Swartz, DA
   Soria, R
   Tennant, AF
   Yukita, M
AF Swartz, Douglas A.
   Soria, Roberto
   Tennant, Allyn F.
   Yukita, Mihoko
TI A COMPLETE SAMPLE OF ULTRALUMINOUS X-RAY SOURCE HOST GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: general; surveys; X-rays: binaries; X-rays: galaxies; X-rays:
   general
ID STAR-FORMATION RATE; MASS BLACK-HOLES; FORMATION RATE INDICATOR;
   TELESCOPE KEY PROJECT; NEARBY GALAXIES; LOCAL UNIVERSE; LUMINOSITY
   FUNCTION; HUBBLE CONSTANT; FORMATION LAW; XMM-NEWTON
AB One hundred seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10(39) erg s(-1) are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 < log(M/M-circle dot) < 11.4, and in star formation rate, 0.0002 < SFR(M-circle dot yr(-1)) <= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10(10) M-circle dot, one per similar to 0.5 M-circle dot yr(-1) star formation rate, and one per 57 Mpc(3) corresponding to a luminosity density of similar to 2 x 10(37) erg s(-1) Mpc(-3). At these rates we estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha similar to -0.8 to -2.0 with an exponential cutoff at similar to 20 x 10(39) erg s(-1) with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L-X similar to 10(41) erg s(-1), within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10(41) erg s(-1), requiring a new population class to explain these extreme objects.
C1 [Swartz, Douglas A.] NASA, Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
   [Soria, Roberto] Curtin Univ, Curtin Inst Radio Astron, Bentley, WA 6102, Australia.
   [Tennant, Allyn F.] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
   [Yukita, Mihoko] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
RP Swartz, DA (reprint author), NASA, Marshall Space Flight Ctr, Univ Space Res Assoc, VP62, Huntsville, AL 35812 USA.
NR 55
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2011
VL 741
IS 1
AR 49
DI 10.1088/0004-637X/741/1/49
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000049
ER

PT J
AU Velusamy, T
   Langer, WD
   Kumar, MSN
   Grave, JMC
AF Velusamy, T.
   Langer, W. D.
   Kumar, M. S. N.
   Grave, J. M. C.
TI JETS AND WIDE-ANGLE OUTFLOWS IN CEPHEUS E: NEW EVIDENCE FROM SPITZER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Herbig-Haro objects; infrared: ISM; ISM: individual objects (Cepheus E);
   ISM: jets and outflows; stars: formation; stars: protostars
ID 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS;
   PROTOSTELLAR SHOCK L1157-B1; YOUNG STELLAR OBJECTS; MOLECULAR-HYDROGEN;
   SCATTERED-LIGHT; STAR-FORMATION; SPACE-TELESCOPE; MASS PROTOSTARS;
   HIGH-VELOCITY
AB Outflows and jets are believed to play a crucial role in determining the mass of the central protostar and its planet-forming disk by virtue of their ability to transport energy, mass, and momentum of the surrounding material, and thus terminate the infall stage in star and disk formation. In some protostellar objects both wide-angle outflows and collimated jets are seen, while in others only one is observed. Spitzer provides unprecedented sensitivity in the infrared to study both the jet and outflow features. Here, we use HiRes deconvolution to improve the visualization of spatial morphology by enhancing resolution (to subarcsecond levels in the Infrared Array Camera (IRAC) bands) and removing the contaminating sidelobes from bright sources. We apply this approach to study the jet and outflow features in Cep E, a young, energetic Class 0 protostar. In the reprocessed images we detect (1) wide-angle outflow seen in scattered light, (2) morphological details on at least 29 jet-driven bow shocks and jet heads or knots, (3) three compact features in 24 mu m continuum image as atomic/ionic line emission coincident with the jet heads, and (4) a flattened similar to 35 '' size protostellar envelope seen against the interstellar background polycyclic aromatic hydrocarbon emission as an absorption band across the protostar at 8 mu m. By separating the protostellar photospheric scattered emission in the wide-angle cavity from the jet emission we show that we can study directly the scattered light spectrum. We present the H-2 emission line spectra, as observed in all IRAC bands, for 29 knots in the jets and bow shocks and use them in the IRAC color-color space as a diagnostic of the thermal gas in the shocks driven by the jets. The data presented here will enable detailed modeling of the individual shocks retracing the history of the episodic jet activity and the associated accretion on to the protostar. The Spitzer data analysis presented here shows the richness of its archive as a resource to study the jet/outflow features in H2 and scattered light in a large homogeneous sample.
C1 [Velusamy, T.; Langer, W. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Kumar, M. S. N.; Grave, J. M. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
RP Velusamy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM velusamy@jpl.nasa.gov; William.D.Langer@jpl.nasa.gov; nanda@astro.up.pt;
   jgrave@astro.up.pt
RI Kumar, Nanda/I-4183-2013; 
OI Grave, Jorge/0000-0003-4897-4595
FU National Aeronautics and Space Administration; Ciencia contract;
   FCT/MCTES (Portugal); POPH/FSE (EC)
FX We thank Dirk Froebrich for useful discussions. We thank the referee,
   Alberto Noriega-Crespo, whose critical comments helped us to present a
   more complete and comprehensive picture of Cep E; in particular, for
   pointing out the presence of a second jet and suggesting using the IRAC
   colors. 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.
   M.S.N.K. is supported by a Ciencia 2007 contract, funded by FCT/MCTES
   (Portugal) and POPH/FSE (EC).
NR 77
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2011
VL 741
IS 1
AR 60
DI 10.1088/0004-637X/741/1/60
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000060
ER

PT J
AU Hermes, JJ
   Mullally, F
   Ostensen, RH
   Williams, KA
   Telting, J
   Southworth, J
   Bloemen, S
   Howell, SB
   Everett, M
   Winget, DE
AF Hermes, J. J.
   Mullally, Fergal
   Ostensen, R. H.
   Williams, Kurtis A.
   Telting, John
   Southworth, John
   Bloemen, S.
   Howell, Steve B.
   Everett, Mark
   Winget, D. E.
TI DISCOVERY OF A ZZ CETI IN THE KEPLER MISSION FIELD
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: individual (WD J191643.83+393849.7); stars: oscillations; stars:
   variables: general; white dwarfs
ID DA WHITE-DWARFS; WHOLE EARTH TELESCOPE; INSTABILITY STRIP; COMPACT
   PULSATORS; LIGHT-CURVE; SKY-SURVEY; STARS; CATALOG
AB We report the discovery of the first identified pulsating DA white dwarf, WD J1916+3938 (Kepler ID 4552982), in the field of the Kepler mission. This ZZ Ceti star was first identified through ground-based, time-series photometry, and follow-up spectroscopy confirms that it is a hydrogen-atmosphere white dwarf with T(eff) = 11,129 +/- 115 K and log g = 8.34 +/- 0.06, placing it within the empirical ZZ Ceti instability strip. The object shows up to 0.5% amplitude variability at several periods between 800 and 1450 s. Extended Kepler observations of WD J1916+3938 could yield the best light curve, to date, of any pulsating white dwarf, allowing us to directly study the interior of an evolved object representative of the fate of the majority of stars in our Galaxy.
C1 [Hermes, J. J.; Winget, D. E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
   [Hermes, J. J.; Winget, D. E.] McDonald Observ, Ft Davis, TX 79734 USA.
   [Mullally, Fergal; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Ostensen, R. H.; Bloemen, S.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
   [Williams, Kurtis A.] Texas A&M Univ Commerce, Dept Phys & Astron, Commerce, TX 75428 USA.
   [Telting, John] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain.
   [Southworth, John] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
   [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM jjhermes@astro.as.utexas.edu
OI Williams, Kurtis/0000-0002-1413-7679
FU Norman Hackerman Advanced Research Program [003658-0255-2007,
   003658-0252-2009]; NASA [NAG5-13094]; National Science Foundation
   [AST-0909107]; European Research Council under the European Community
   [227224]; Research Council of K.U. Leuven [GOA/2008/04]
FX We thank KASC WG11 for their enthusiasm, especially regarding
   spectroscopic follow-ups. This work is supported by the Norman Hackerman
   Advanced Research Program, under grants 003658-0255-2007 and
   003658-0252-2009, by a grant from the NASA Origins Program, NAG5-13094,
   and by the National Science Foundation, under grant AST-0909107. The
   research leading to these results has received funding from the European
   Research Council under the European Community's Seventh Framework
   Programme (FP7/2007-2013)/ERC grant agreement n degrees 227224
   (PROSPERITY), as well as from the Research Council of K.U. Leuven grant
   agreement GOA/2008/04. This work was partly based on observations made
   with the Nordic Optical Telescope, operated on the island of La Palma
   jointly by Denmark, Finland, Iceland, Norway, and Sweden. We thank the
   McDonald Observatory staff for their support, especially Dave Doss and
   John Kuehne.
NR 31
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U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 1
PY 2011
VL 741
IS 1
AR L16
DI 10.1088/2041-8205/741/1/L16
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844NC
UT WOS:000296753000016
ER

PT J
AU Striani, E
   Tavani, M
   Piano, G
   Donnarumma, I
   Pucella, G
   Vittorini, V
   Bulgarelli, A
   Trois, A
   Pittori, C
   Verrecchia, F
   Costa, E
   Weisskopf, M
   Tennant, A
   Argan, A
   Barbiellini, G
   Caraveo, P
   Cardillo, M
   Cattaneo, PW
   Chen, AW
   De Paris, G
   Del Monte, E
   Di Cocco, G
   Evangelista, Y
   Ferrari, A
   Feroci, M
   Fuschino, F
   Galli, M
   Gianotti, F
   Giuliani, A
   Labanti, C
   Lapshov, I
   Lazzarotto, F
   Longo, F
   Marisaldi, M
   Mereghetti, S
   Morselli, A
   Pacciani, L
   Pellizzoni, A
   Perotti, F
   Picozza, P
   Pilia, M
   Rapisarda, M
   Rappoldi, A
   Sabatini, S
   Soffitta, P
   Trifoglio, M
   Vercellone, S
   Lucarelli, F
   Santolamazza, P
   Giommi, P
AF Striani, E.
   Tavani, M.
   Piano, G.
   Donnarumma, I.
   Pucella, G.
   Vittorini, V.
   Bulgarelli, A.
   Trois, A.
   Pittori, C.
   Verrecchia, F.
   Costa, E.
   Weisskopf, M.
   Tennant, A.
   Argan, A.
   Barbiellini, G.
   Caraveo, P.
   Cardillo, M.
   Cattaneo, P. W.
   Chen, A. W.
   De Paris, G.
   Del Monte, E.
   Di Cocco, G.
   Evangelista, Y.
   Ferrari, A.
   Feroci, M.
   Fuschino, F.
   Galli, M.
   Gianotti, F.
   Giuliani, A.
   Labanti, C.
   Lapshov, I.
   Lazzarotto, F.
   Longo, F.
   Marisaldi, M.
   Mereghetti, S.
   Morselli, A.
   Pacciani, L.
   Pellizzoni, A.
   Perotti, F.
   Picozza, P.
   Pilia, M.
   Rapisarda, M.
   Rappoldi, A.
   Sabatini, S.
   Soffitta, P.
   Trifoglio, M.
   Vercellone, S.
   Lucarelli, F.
   Santolamazza, P.
   Giommi, P.
TI THE CRAB NEBULA SUPER-FLARE IN 2011 APRIL: EXTREMELY FAST PARTICLE
   ACCELERATION AND GAMMA-RAY EMISSION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; gamma rays: stars; pulsars: individual (Crab
   Nebula)
ID SYNCHROTRON NEBULA; STANDARD CANDLE; SHOCKS; SIMULATIONS; DISCOVERY;
   TELESCOPE
AB We report on the extremely intense and fast gamma-ray flare above 100 MeV detected by AGILE from the Crab Nebula in mid-April 2011. This event is the fourth of a sequence of reported major gamma-ray flares produced by the Crab Nebula in the period 2007/mid-2011. These events are attributed to strong radiative and plasma instabilities in the inner Crab Nebula, and their properties are crucial for theoretical studies of fast and efficient particle acceleration up to 10(15) eV. Here we study the very rapid flux and spectral evolution of the event that on 2011 April 16 reached the record-high peak flux of F = (26 +/- 5) x 10(-6) photons cm(-2) s(-1) with a rise-time timescale that we determine to be in the range 6-10 hr. The peak flaring gamma-ray spectrum reaches a distinct maximum near 500 MeV with no substantial emission above 1 GeV. The very rapid rise time and overall evolution of the Crab Nebula flare strongly constrain the acceleration mechanisms and challenge MHD models. We briefly discuss the theoretical implications of our observations.
C1 [Striani, E.; Tavani, M.; Cardillo, M.; Picozza, P.] Univ Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
   [Tavani, M.; Piano, G.; Donnarumma, I.; Vittorini, V.; Trois, A.; Costa, E.; Argan, A.; Cardillo, M.; De Paris, G.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Sabatini, S.; Soffitta, P.] INAF IASF Roma, I-00133 Rome, Italy.
   [Pucella, G.; Rapisarda, M.] ENEA Frascati, I-00044 Rome, Italy.
   [Bulgarelli, A.] INFN Roma La Sapienza, I-00185 Rome, Italy.
   [Pittori, C.; Verrecchia, F.; Lucarelli, F.; Santolamazza, P.; Giommi, P.] ASI Sci Data Ctr, I-00044 Rome, Italy.
   [Weisskopf, M.; Tennant, A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 36812 USA.
   [Barbiellini, G.; Longo, F.] Dipartimento Fis, I-34127 Trieste, Italy.
   [Barbiellini, G.; Longo, F.] INFN Trieste, I-34127 Trieste, Italy.
   [Caraveo, P.; Chen, A. W.; Giuliani, A.; Mereghetti, S.; Perotti, F.] INAF IASF Milano, I-20133 Milan, Italy.
   [Cattaneo, P. W.; Rappoldi, A.] INFN Pavia, I-27100 Pavia, Italy.
   [Chen, A. W.; Ferrari, A.] CIFS Torino, I-10133 Turin, Italy.
   [Di Cocco, G.; Fuschino, F.; Gianotti, F.; Labanti, C.; Marisaldi, M.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
   [Ferrari, A.] Univ Turin, Dipartimento Fis, Turin, Italy.
   [Galli, M.] ENEA Bologna, I-40129 Bologna, Italy.
   [Morselli, A.; Picozza, P.] INFN Roma Tor Vergata, I-00133 Rome, Italy.
   [Pellizzoni, A.; Pilia, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy.
   [Vercellone, S.] INAF IASF Palermo, Palermo, Italy.
   CNR IMIP, Rome, Italy.
   Univ Insubria, Dipartimento Fis, I-22100 Como, Italy.
RP Striani, E (reprint author), Univ Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RI Lazzarotto, Francesco/J-4670-2012; Morselli, Aldo/G-6769-2011;
   Trifoglio, Massimo/F-5302-2015; Pittori, Carlotta/C-7710-2016; 
OI Marisaldi, Martino/0000-0002-4000-3789; Vercellone,
   Stefano/0000-0003-1163-1396; MEREGHETTI, SANDRO/0000-0003-3259-7801;
   Tavani, Marco/0000-0003-2893-1459; Lucarelli,
   Fabrizio/0000-0002-6311-764X; Labanti, Claudio/0000-0002-5086-3619;
   Feroci, Marco/0000-0002-7617-3421; Soffitta, Paolo/0000-0002-7781-4104;
   Picozza, Piergiorgio/0000-0002-7986-3321; Fuschino,
   Fabio/0000-0003-2139-3299; Caraveo, Patrizia/0000-0003-2478-8018;
   Verrecchia, Francesco/0000-0003-3455-5082; Gianotti,
   Fulvio/0000-0003-4666-119X; Lazzarotto, Francesco/0000-0003-4871-4072;
   Costa, Enrico/0000-0003-4925-8523; Donnarumma,
   Immacolata/0000-0002-4700-4549; Sabatini, Sabina/0000-0003-2076-5767;
   Morselli, Aldo/0000-0002-7704-9553; Trifoglio,
   Massimo/0000-0002-2505-3630; Pittori, Carlotta/0000-0001-6661-9779;
   Bulgarelli, Andrea/0000-0001-6347-0649; galli,
   marcello/0000-0002-9135-3228; Pacciani, Luigi/0000-0001-6897-5996;
   giommi, paolo/0000-0002-2265-5003; trois, alessio/0000-0002-3180-6002;
   Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Cardillo,
   Martina/0000-0001-8877-3996
FU ASI [I/042/10/0]
FX Research partially supported by ASI grant No. I/042/10/0.
NR 37
TC 35
Z9 35
U1 0
U2 15
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 1
PY 2011
VL 741
IS 1
AR L5
DI 10.1088/2041-8205/741/1/L5
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844NC
UT WOS:000296753000005
ER

PT J
AU Winn, JN
   Albrecht, S
   Johnson, JA
   Torres, G
   Cochran, WD
   Marcy, GW
   Howard, AW
   Isaacson, H
   Fischer, D
   Doyle, L
   Welsh, W
   Carter, JA
   Fabrycky, DC
   Ragozzine, D
   Quinn, SN
   Shporer, A
   Howell, SB
   Latham, DW
   Orosz, J
   Prsa, A
   Slawson, RW
   Borucki, WJ
   Koch, D
   Barclay, T
   Boss, AP
   Christensen-Dalsgaard, J
   Girouard, FR
   Jenkins, J
   Klaus, TC
   Meibom, S
   Morris, RL
   Sasselov, D
   Still, M
   Van Cleve, J
AF Winn, Joshua N.
   Albrecht, Simon
   Johnson, John Asher
   Torres, Guillermo
   Cochran, William D.
   Marcy, Geoffrey W.
   Howard, Andrew W.
   Isaacson, Howard
   Fischer, Debra
   Doyle, Laurance
   Welsh, William
   Carter, Joshua A.
   Fabrycky, Daniel C.
   Ragozzine, Darin
   Quinn, Samuel N.
   Shporer, Avi
   Howell, Steve B.
   Latham, David W.
   Orosz, Jerome
   Prsa, Andrej
   Slawson, Robert W.
   Borucki, William J.
   Koch, David
   Barclay, Thomas
   Boss, Alan P.
   Christensen-Dalsgaard, Jorgen
   Girouard, Forrest R.
   Jenkins, Jon
   Klaus, Todd C.
   Meibom, Soren
   Morris, Robert L.
   Sasselov, Dimitar
   Still, Martin
   Van Cleve, Jeffrey
TI SPIN-ORBIT ALIGNMENT FOR THE CIRCUMBINARY PLANET HOST KEPLER-16 A
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: general; planets and satellites: formation; stars: individual
   (Kepler-16 A, KIC 12644769); stars: low-mass; stars: rotation
ID LOWER MAIN-SEQUENCE; CLOSE BINARY-SYSTEMS; LOW-MASS STARS; ECLIPSING
   BINARY; ABSOLUTE DIMENSIONS; EVOLUTIONARY MODELS; HIERARCHICAL TRIPLE;
   BROWN DWARF; ROTATION; STELLAR
AB Kepler-16 is an eccentric low-mass eclipsing binary with a circumbinary transiting planet. Here, we investigate the angular momentum of the primary star, based on Kepler photometry and Keck spectroscopy. The primary star's rotation period is 35.1 +/- 1.0 days, and its projected obliquity with respect to the stellar binary orbit is 1.degrees 6 +/- 2.degrees 4. Therefore, the three largest sources of angular momentum-the stellar orbit, the planetary orbit, and the primary's rotation-are all closely aligned. This finding supports a formation scenario involving accretion from a single disk. Alternatively, tides may have realigned the stars despite their relatively wide separation (0.2 AU), a hypothesis that is supported by the agreement between the measured rotation period and the "pseudosynchronous" period of tidal evolution theory. The rotation period, chromospheric activity level, and fractional light variations suggest a main-sequence age of 2-4 Gyr. Evolutionary models of low-mass stars can match the observed masses and radii of the primary and secondary stars to within about 3%.
C1 [Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Cambridge, MA 02139 USA.
   [Winn, Joshua N.; Albrecht, Simon] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
   [Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
   [Johnson, John Asher] NASA Exoplanet Sci Inst NExScI, Pasadena, CA USA.
   [Torres, Guillermo; Carter, Joshua A.; Ragozzine, Darin; Quinn, Samuel N.; Latham, David W.; Meibom, Soren; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
   [Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
   [Doyle, Laurance; Slawson, Robert W.; Jenkins, Jon; Morris, Robert L.; Van Cleve, Jeffrey] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA.
   [Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
   [Welsh, William; Orosz, Jerome] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
   [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
   [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
   [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
   [Boss, Alan P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
   [Christensen-Dalsgaard, Jorgen] Aarhus Univ, Danish AsteroSeismol Ctr, DK-8000 Aarhus C, Denmark.
   [Christensen-Dalsgaard, Jorgen] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
   [Girouard, Forrest R.; Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Howard,
   Andrew/D-4148-2015; 
OI Howard, Andrew/0000-0001-8638-0320; Barclay, Thomas/0000-0001-7139-2724;
   Fabrycky, Daniel/0000-0003-3750-0183
FU NASA [NNX09AB33G]; NSF [AST-1007992]; W. M. Keck Foundation
FX We thank Brice-Olivier Demory, Nevin Weinberg, and Jamie Lloyd for
   helpful discussions. Work by J.N.W. and S.A. was supported by NASA
   Origins award NNX09AB33G. G.T. acknowledges partial support from the NSF
   through grant AST-1007992. Funding for the Kepler Discovery mission is
   provided by NASA's Science Mission Directorate. The W. M. Keck
   Observatory is operated as a scientific partnership among the California
   Institute of Technology, the University of California, and the National
   Aeronautics and Space Administration, and was made possible by the
   generous financial support of the W. M. Keck Foundation. We extend
   special thanks to those of Hawaiian ancestry on whose sacred mountain of
   Mauna Kea we are privileged to be guests.
NR 47
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U1 1
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 1
PY 2011
VL 741
IS 1
AR L1
DI 10.1088/2041-8205/741/1/L1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844NC
UT WOS:000296753000001
ER

PT J
AU Nakamura, M
   Meier, DL
   Garofalo, D
AF Nakamura, M.
   Meier, D. L.
   Garofalo, D.
TI Magnetohydrodynamic properties of extragalactic jets
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article
DE Active galaxies; Jets galaxies; Numerical methods; MHD
ID M87 JET; BLACK-HOLE; NUMERICAL SIMULATIONS; RELATIVISTIC JETS;
   HIGH-RESOLUTION; EMISSION; CENTIMETERS; DYNAMICS; MOTIONS; HST-1
AB The theory that magnetic fields are instrumental in the formation and propagation of jets in active galactic nuclei dates back four decades. Despite a recent growing consensus on this notion stemming from the results of numerical simulations of magnetohydrodynamic (MHD) flows near black holes, the precise dynamical role of magnetic fields in observed parsec and kiloparsec jets remains uncertain. Some of the unanswered fundamental questions about extragalactic jets include the location where the flow becomes relativistic and where acceleration and collimation terminate, as well as the specifics of how the flow interacts with the ISM. Such observed properties as superluminal motions and wiggled structures based on numerical simulations to constitute the foundation of an MHD paradigm for extragalactic jets. We particularly focus our attention to the M87 jet, which is one of the best candidates to investigate relativistic outflows in extragalactic system.
C1 [Nakamura, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
   [Nakamura, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Meier, D. L.; Garofalo, D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Nakamura, M (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM nakamura@pha.jhu.edu
FU Department of Physics and Astronomy at Johns Hopkins University; Space
   Telescope Science Institute; National Aeronautics and Space
   Administration
FX Stimulating discussions with Colin A. Norman and Keiichi Asada are
   gratefully acknowledged. M.N. is supported by the Allan C. Davis
   fellowship jointly awarded by the Department of Physics and Astronomy at
   Johns Hopkins University and the Space Telescope Science Institute. Part
   of this research described was carried out at the Jet Propulsion
   Laboratory, California Institute of Technology, under contract to the
   National Aeronautics and Space Administration.
NR 40
TC 1
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U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
EI 1572-946X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD NOV
PY 2011
VL 336
IS 1
BP 15
EP 19
DI 10.1007/s10509-010-0490-z
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844EZ
UT WOS:000296731800004
ER

PT J
AU Dorodnitsyn, A
   Kallman, T
AF Dorodnitsyn, A.
   Kallman, T.
TI X-ray polarization signature of warm absorber winds in AGN
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article
DE Acceleration of particles; Galaxies: active; Hydrodynamics; Methods:
   numerical; Quasars: absorption lines; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; REFLECTION GRATING SPECTROMETER; HYDRODYNAMICAL
   MODEL; SEYFERT-GALAXIES; LINE FORMATION; TORUS WIND; NGC 5548;
   RADIATION; FLOWS; EMISSION
AB Accretion onto a supermassive black hole in Active Galactic Nuclei (AGN), Seyfert galaxies and quasars is often accompanied by winds which are powerful enough to affect the AGN mass budget, and whose observational appearance bears an imprint of processes which are happening within the central parsec around the black hole (BH). One example of such a wind is the partially ionized gas responsible for X-ray and UV absorption ('warm absorbers'). Here we perform 3D calculations of transfer of polarized light in 0.1-10 keV range from hydrodynamical model of warm absorber flow and show that such gas will have a distinct signature when viewed in polarized X-rays and it will be detectable by future dedicated X-ray polarimetry space missions, such as the NASA Gravity and Extreme Magnetism SMEX, GEMS.
C1 [Dorodnitsyn, A.; Kallman, T.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
RP Dorodnitsyn, A (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
EM dora@milkyway.gsfc.nasa.gov
FU NASA Goddard Space Flight Center; NASA [05-ATP05-18]
FX This research was supported by an appointment at the NASA Goddard Space
   Flight Center, administered by CRESST/UMD through a contract with NASA,
   and by grants from the NASA Astrophysics Theory Program 05-ATP05-18.
NR 38
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U1 1
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD NOV
PY 2011
VL 336
IS 1
BP 245
EP 250
DI 10.1007/s10509-011-0656-3
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844EZ
UT WOS:000296731800040
ER

PT J
AU Dotson, KT
   Sunderland, PB
   Yuan, ZG
   Urban, DL
AF Dotson, K. T.
   Sunderland, P. B.
   Yuan, Z. -G.
   Urban, D. L.
TI Laminar smoke points of coflowing flames in microgravity
SO FIRE SAFETY JOURNAL
LA English
DT Article
DE Combustion; Laminar gas jet diffusion flames; Residence time; Soot
ID JET DIFFUSION FLAMES; SOOT FORMATION; HYDRODYNAMIC SUPPRESSION;
   HYDROCARBON FLAMES; MODEL; VELOCITY; SHAPES; FUELS; AIR; PREDICTION
AB Laminar smoke points were measured in nonbuoyant laminar jet diffusion flames in coflowing air. Microgravity was obtained on board the International Space Station. A total of 55 smoke points were found for ethylene, propane, propylene, and propylene/nitrogen mixtures. Burner diameters were 0.41, 0.76, and 1.6 mm, and coflow velocities varied from 5.4 to 65 cm/s. These flames allow extensive control over residence time via variations in dilution, burner diameter, and coflow velocity. The measured smoke-point lengths scaled with d(-0.91)u(air)(0.41), where d is burner diameter and u(air) is coflow velocity. The measurements yielded estimates of sooting propensities of the present fuels in microgravity diffusion flames. Analytical models of residence times in gas jet flames are presented, and although residence time helps explain many of the observed trends it does not correlate the measured smoke points. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Dotson, K. T.; Sunderland, P. B.] Univ Maryland, Dept Fire Protect Engn, College Pk, MD 20742 USA.
   [Yuan, Z. -G.] Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
   [Urban, D. L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Sunderland, PB (reprint author), Univ Maryland, Dept Fire Protect Engn, 3104 JM Patterson Bldg, College Pk, MD 20742 USA.
EM pbs@umd.edu
OI Sunderland, Peter/0000-0002-8262-7100
FU NASA [NNX07-AO91A]; Department of Fire Protection Engineering
FX Work at the University of Maryland was supported by NASA cooperative
   agreement NNX07-AO91A and the Department of Fire Protection Engineering.
   The authors acknowledge G.M. Faeth for conceiving this work, M.A.
   Delichatsios for help with residence times, the SPICE engineering team
   for building the hardware, and astronauts M. Barratt, E.M. Fincke, S.H.
   Magnus, and K. Wakata for conducting the tests.
NR 39
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U1 0
U2 12
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0379-7112
J9 FIRE SAFETY J
JI Fire Saf. J.
PD NOV
PY 2011
VL 46
IS 8
BP 550
EP 555
DI 10.1016/j.firesaf.2011.08.002
PG 6
WC Engineering, Civil; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 843OP
UT WOS:000296682000008
ER

PT J
AU Li, LM
   Jiang, X
   Ingersoll, AP
   Del Genio, AD
   Porco, CC
   West, RA
   Vasavada, AR
   Ewald, SP
   Conrath, BJ
   Gierasch, PJ
   Simon-Miller, AA
   Nixon, CA
   Achterberg, RK
   Orton, GS
   Fletcher, LN
   Baines, KH
AF Li, Liming
   Jiang, Xun
   Ingersoll, Andrew P.
   Del Genio, Anthony D.
   Porco, Carolyn C.
   West, Robert A.
   Vasavada, Ashwin R.
   Ewald, Shawn P.
   Conrath, Barney J.
   Gierasch, Peter J.
   Simon-Miller, Amy A.
   Nixon, Conor A.
   Achterberg, Richard K.
   Orton, Glenn S.
   Fletcher, Leigh N.
   Baines, Kevin H.
TI Equatorial winds on Saturn and the stratospheric oscillation
SO NATURE GEOSCIENCE
LA English
DT Article
ID CLOUD LEVEL; JUPITER; JET; TEMPERATURES; ATMOSPHERE
AB The zonal jets on the giant planets have been thought to be stable in time(1-3). A decline in the velocity of Saturn's equatorial jet has been identified, on the basis of a comparison of cloud-tracking data across two decades(4), but the differences in cloud speeds have since been suggested to stem from changes in cloud altitude in combination with vertical wind shear, rather than from temporal changes in wind strength at a given height(5). Here, we combine observations of cloud tracks and of atmospheric temperatures taken by two instruments on the Cassini spacecraft to reveal a significant temporal variation in the strength of the high-altitude equatorial jet on Saturn. Specifically, we find that wind speeds at atmospheric pressure levels of 60 mbar, corresponding to Saturn's tropopause, increased by about 20m s(-1) between 2004 and 2008, whereas the wind speed has been essentially constant over time in the southern equatorial troposphere. The observations further reveal that the equatorial jet intensified by about 60m s(-1) between 2005 and 2008 in the stratosphere, that is, at pressure levels of 1-5 mbar. Because the wind acceleration is weaker near the tropopause than higher up, in the stratosphere, we conclude that the semi-annual equatorial oscillation of Saturn's middle atmosphere(6,7) is also damped as it propagates downwards.
C1 [Li, Liming; Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
   [Ingersoll, Andrew P.; Ewald, Shawn P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Porco, Carolyn C.] CICLOPS Space Sci Inst, Boulder, CO 80301 USA.
   [West, Robert A.; Vasavada, Ashwin R.; Orton, Glenn S.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Conrath, Barney J.; Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Nixon, Conor A.; Achterberg, Richard K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Fletcher, Leigh N.] Univ Oxford, Oxford OX1 3PU, England.
RP Li, LM (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
EM lli7@mail.uh.edu
RI Nixon, Conor/A-8531-2009; Del Genio, Anthony/D-4663-2012; Fletcher,
   Leigh/D-6093-2011; Simon, Amy/C-8020-2012
OI Nixon, Conor/0000-0001-9540-9121; Del Genio,
   Anthony/0000-0001-7450-1359; Fletcher, Leigh/0000-0001-5834-9588; Simon,
   Amy/0000-0003-4641-6186
FU NASA
FX NASA Cassini Data Analysis Program funded this work. We acknowledge E.
   Garcia-Melendo, R. Hueso, A. Sanchez-Lavega, and S. Perez-Hoyos for
   providing comments and discussions. We are also grateful for comments
   and suggestions on this work from two anonymous reviewers.
NR 22
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Z9 4
U1 0
U2 9
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD NOV
PY 2011
VL 4
IS 11
BP 750
EP 752
DI 10.1038/NGEO1292
PG 3
WC Geosciences, Multidisciplinary
SC Geology
GA 844BW
UT WOS:000296723500010
ER

PT J
AU Ding, LB
   Kowalewski, MG
   Cooper, JW
   Smith, GR
   Barnes, RA
   Waluschka, E
   Butler, JJ
AF Ding, Leibo
   Kowalewski, Matthew G.
   Cooper, John W.
   Smith, Gilbert R.
   Barnes, Robert A.
   Waluschka, Eugene
   Butler, James J.
TI Development and performance of a filter radiometer monitor system for
   integrating sphere sources
SO OPTICAL ENGINEERING
LA English
DT Article
DE integrating sphere; calibration; stability; radiometer
ID EARTH OBSERVING SYSTEM; CALIBRATION
AB The NASA Goddard Space Flight Center (GSFC) Radiometric Calibration Laboratory (RCL) maintains several large integrating sphere sources covering the visible to the shortwave infrared wavelength range. Two critical, functional requirements of an integrating sphere source are short- and long-term operational stability and repeatability. Monitoring the source is essential in determining the origin of systemic errors, thus increasing confidence in source performance and quantifying repeatability. If monitor data falls outside the established parameters, this could be an indication that the source requires maintenance or recalibration against the National Institute of Science and Technology irradiance standard. The GSFC RCL has developed a Filter Radiometer Monitoring System (FRMS) to continuously monitor the performance of its integrating sphere calibration sources in the 400 to 2400 nm region. Sphere output change mechanisms include lamp aging, coating (e.g., BaSO(4)) deterioration, and ambient water vapor level. The FRMS wavelength bands are selected to quantify changes caused by these mechanisms. The FRMS design and operation are presented, as well as data from monitoring four of the RCL's integrating sphere sources. (C) 2011 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.3646532]
C1 [Ding, Leibo; Cooper, John W.; Smith, Gilbert R.] SigmaSpace Corp, Lanham, MD 20706 USA.
   [Kowalewski, Matthew G.] Univ Space Res Org, Columbia, MD 21044 USA.
   [Barnes, Robert A.] Sci Applicat Int Corp, Beltsville, MD 20705 USA.
   [Waluschka, Eugene; Butler, James J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ding, LB (reprint author), SigmaSpace Corp, Lanham, MD 20706 USA.
RI Butler, James/D-4188-2013
NR 7
TC 1
Z9 1
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 NOV
PY 2011
VL 50
IS 11
AR 113603
DI 10.1117/1.3646532
PG 12
WC Optics
SC Optics
GA 847KK
UT WOS:000296971600023
ER

PT J
AU Yan, Y
   Wang, J
   Zhang, L
   Yang, JY
   Fazal, IM
   Ahmed, N
   Shamee, B
   Willner, AE
   Birnbaum, K
   Dolinar, S
AF Yan, Yan
   Wang, Jian
   Zhang, Lin
   Yang, Jeng-Yuan
   Fazal, Irfan M.
   Ahmed, Nisar
   Shamee, Bishara
   Willner, Alan E.
   Birnbaum, Kevin
   Dolinar, Sam
TI Fiber coupler for generating orbital angular momentum modes
SO OPTICS LETTERS
LA English
DT Article
ID LIGHT; BEAMS
AB We propose a fiber coupler consisting of a central ring and four external cores to generate up to ten orbital angular momentum (OAM) modes. Four coherent input lights are launched into the external cores and then coupled into the central ring waveguide to generate OAM modes. By changing the size of the external cores, one can selectively excite a high-order OAM mode. The quality of the generated OAM modes can be enhanced by adjusting the polarization state and the phase of input lights. We show the generation of OAM modes with odd charge numbers of -9 to +9 (i.e., 10 modes totally) with mode purity of >99% using <2mm long fiber. This fiber coupler design can be extended to enable all-fiber spatial-mode (de) multiplexing. (C) 2011 Optical Society of America
C1 [Yan, Yan; Wang, Jian; Zhang, Lin; Yang, Jeng-Yuan; Fazal, Irfan M.; Ahmed, Nisar; Shamee, Bishara; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
   [Birnbaum, Kevin; Dolinar, Sam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yan, Y (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
EM yanyan@usc.edu
RI Zhang, Lin/E-7913-2011
OI Zhang, Lin/0000-0003-0545-1110
FU Defense Advanced Research Projects Agency (DARPA)
FX We acknowledge the support of the Defense Advanced Research Projects
   Agency (DARPA) under the InPho program. We are thankful for the fruitful
   discussion with Prof. Moshe Tur at Tel Aviv University, Israel.
NR 10
TC 27
Z9 28
U1 3
U2 37
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 1
PY 2011
VL 36
IS 21
BP 4269
EP 4271
PG 3
WC Optics
SC Optics
GA 844GC
UT WOS:000296734700050
PM 22048387
ER

PT J
AU Porikli, F
   Al Bovik
   Plack, C
   AlRegib, G
   Farrell, J
   Le Callet, P
   Quan, HT
   Moller, S
   Winkler, S
AF Porikli, Fatih
   Al Bovik
   Plack, Chris
   AlRegib, Ghassan
   Farrell, Joyce
   Le Callet, Patrick
   Quan Huynh-Thu
   Moeller, Sebastian
   Winkler, Stefan
TI Multimedia Quality Assessment
SO IEEE SIGNAL PROCESSING MAGAZINE
LA English
DT Editorial Material
C1 [Porikli, Fatih] MERL, Cambridge, MA USA.
   [Al Bovik] Univ Texas Austin, LIVE, Dept Elect & Comp Engn, Austin, TX 78712 USA.
   [Al Bovik] Univ Texas Austin, Inst Neurosci, Austin, TX 78712 USA.
   [Plack, Chris] Univ Manchester, Manchester M13 9PL, Lancs, England.
   [AlRegib, Ghassan] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
   [Farrell, Joyce] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
   [Farrell, Joyce] Stanford Ctr Image Syst Engn, Stanford, CA USA.
   [Farrell, Joyce] NASA, Ames Res Ctr, Washington, DC 20546 USA.
   [Farrell, Joyce] NYU, New York, NY 10003 USA.
   [Farrell, Joyce] Xerox Palo Alto Res Ctr, Palo Alto, CA USA.
   [Farrell, Joyce] Hewlett Packard Labs, Mississauga, ON, Canada.
   [Le Callet, Patrick] Univ Nantes, Polytech Nantes, F-44035 Nantes, France.
   [Le Callet, Patrick] CNRS IRCCyN, Image & Video Commun Grp, Paris, France.
   [Moeller, Sebastian] TU Berlin, Deutsch Telekom Labs, Berlin, Germany.
   [Winkler, Stefan] Univ Illinois, Adv Digital Sci Ctr, Singapore, Singapore.
RP Porikli, F (reprint author), MERL, Cambridge, MA USA.
EM fatih@merl.com; bovik@ece.utexas.edu; Chris.Plack@manchester.ac.uk;
   alregib@gatech.edu; joyce_farrell@stan-ford.edu;
   patrick.lecallet@univ-nantes.fr; qht@ieee.org;
   sebastian.moeller@telekom.de; stefan.winkler@adsc.com.sg
RI Magazine, Signal Processing/E-9947-2015; 
OI Plack, Christopher/0000-0002-2987-5332
NR 0
TC 8
Z9 8
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1053-5888
J9 IEEE SIGNAL PROC MAG
JI IEEE Signal Process. Mag.
PD NOV
PY 2011
VL 28
IS 6
BP 164
EP 177
DI 10.1109/MSP.2011.942341
PG 14
WC Engineering, Electrical & Electronic
SC Engineering
GA 840UF
UT WOS:000296466100019
ER

PT J
AU Mulenburg, G
AF Mulenburg, Gerald
TI Managing
SO JOURNAL OF PRODUCT INNOVATION MANAGEMENT
LA English
DT Book Review
C1 [Mulenburg, Gerald] NASA, Washington, DC USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0737-6782
J9 J PROD INNOVAT MANAG
JI J. Prod. Innov. Manage.
PD NOV
PY 2011
VL 28
IS 6
SI SI
BP 988
EP 989
PG 2
WC Business; Engineering, Industrial; Management
SC Business & Economics; Engineering
GA 841XA
UT WOS:000296547300013
ER

PT J
AU Kirkpatrick, C
   McCaul, EW
   Cohen, C
AF Kirkpatrick, Cody
   McCaul, Eugene W., Jr.
   Cohen, Charles
TI Sensitivities of Simulated Convective Storms to Environmental CAPE
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID TORNADO FORECAST PARAMETERS; VERTICAL WIND SHEAR; RAPID UPDATE CYCLE;
   PRECIPITATION EFFICIENCY; PROXIMITY SOUNDINGS; SUPERCELL STORMS; SQUALL
   LINE; MIXED-LAYER; THUNDERSTORM; CLIMATOLOGY
AB A set of 225 idealized three-dimensional cloud-resolving simulations is used to explore convective storm behavior in environments with various values of CAPE (450, 800, 2000, and 3200 J kg(-1)). The simulations show that when CAPE = 2000 J kg(-1) or greater, numerous combinations of other environmental parameters can support updrafts of at least 10 m s(-1) throughout an entire 2-h simulation. At CAPE = 450 J kg(-1), it is very difficult to obtain strong storms, although one case featuring a supercell is found. For CAPE = 800 J kg(-1), mature storm updraft speeds correlate positively with strong low-level lapse rates and reduced precipitable water. In some cases, updrafts at this CAPE value can reach speeds that rival predictions of parcel theory, but such efficient conversion of CAPE to kinetic energy does not extend to all storms at CAPE = 800 J kg(-1), nor to any storms in simulations at lower or higher CAPE. In simulations with CAPE = 2000 or 3200 J kg(-1). the strongest time-averaged mature updrafts, while supercellular in character, feature generally less than 60% of the speeds expected from parcel theory, and even the strongest updraft found at CAPE = 450 J kg(-1) fails to reach that relative strength. When CAPE = 2000 J kg(-1) or more, updrafts benefit from enhanced shear, higher levels of free convection, and reduced precipitable water.
   Strong low-level shear and a reduced height of the level of free convection correlate closely with low-level storm vertical vorticity when CAPE is at least 2000 J kg(-1), consistent with previous findings. However, at CAPE = 800 J kg(-1), low-level vorticity shares the same correlations with the environment as updraft strength. With respect to storm precipitation, in simulations initiated with only 30 mm of precipitable water (PW), all of the storms that last for an entire 2-h simulation tend to produce liquid precipitation at roughly similar rates, regardless of their CAPE. In environments where PW is increased to 60 mm, storms tend to produce the most rainfall at CAPE = 2000 J kg(-1), with somewhat lesser rainfall rates at lower and higher CAPE. Nevertheless, over the simulation domain, the ground area that receives at least 10 mm of rainfall tends to increase as CAPE increases, owing to a greater number and size of precipitating updrafts in the domain.
C1 [Kirkpatrick, Cody] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA.
   [McCaul, Eugene W., Jr.; Cohen, Charles] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
RP Kirkpatrick, C (reprint author), UCAR COMET, POB 3000, Boulder, CO 80307 USA.
EM codyk@ucar.edu
FU National Oceanic and Atmospheric Administration (NOAA) at UA Huntsville
   [NA08OAR4600896]; National Science Foundation [ATM-0126408]
FX This research was supported by a grant from the National Oceanic and
   Atmospheric Administration (NOAA) to Dr. Kevin Knupp at UA Huntsville
   (Grant NA08OAR4600896). Publication support was provided by the Earth
   System Science Center at UA Huntsville. We appreciate the detailed
   reviews provided by Dr. David Schultz (Chief Editor), Stephen Corfidi,
   and three additional anonymous reviewers; their constructive criticisms
   have resulted in a greatly improved manuscript. We acknowledge computing
   support from Scott Podgorny (UAH) and Jayanthi Srikishen of USRA in
   Huntsville. Original support for the COMPASS simulations was provided in
   2002 through Grant ATM-0126408 from the National Science Foundation,
   under the supervision of Dr. Stephan Nelson. (For additional
   information, please see the COMPASS Web site at
   http://space.hsv.usra.edu/COMPASS/.)
NR 67
TC 8
Z9 9
U1 0
U2 14
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 NOV
PY 2011
VL 139
IS 11
BP 3514
EP 3532
DI 10.1175/2011MWR3631.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 840XP
UT WOS:000296475700010
ER

PT J
AU Waligorski, MPR
   Cucinotta, FA
AF Waligorski, Michael P. R.
   Cucinotta, Francis A.
TI Robert Katz (1917-2011) IN MEMORIAM
SO RADIATION RESEARCH
LA English
DT Biographical-Item
ID HEAVY ION BOMBARDMENT
C1 [Waligorski, Michael P. R.] Polish Acad Sci, Inst Nucl Phys, PL-31342 Krakow, Poland.
   [Waligorski, Michael P. R.] Ctr Oncol, PL-31115 Krakow, Poland.
   [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Waligorski, MPR (reprint author), Polish Acad Sci, Inst Nucl Phys, PL-31342 Krakow, Poland.
NR 6
TC 0
Z9 0
U1 0
U2 1
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 NOV
PY 2011
VL 176
IS 5
BP 692
EP 693
DI 10.1667/RR2777.1
PG 2
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
   Nuclear Medicine & Medical Imaging
GA 841VZ
UT WOS:000296544600015
PM 22026717
ER

PT J
AU Nicogossian, AE
   Doarn, CR
AF Nicogossian, Arnauld E.
   Doarn, Charles R.
TI Armenia 1988 Earthquake and Telemedicine: Lessons Learned and Forgotten
SO TELEMEDICINE AND E-HEALTH
LA English
DT Article
DE disasters; chronic diseases; acutemedical and public health problems;
   telemedicine; information technology; medical and health networks;
   preparedness planning; chronic metabolic disorders; PTSD
ID SPACE PROGRAM; TELECOMMUNICATIONS; DISORDER; MEDICINE
AB Purpose: To showcase the observations and lessons learned from the first large-scale international telemedicine program addressing the medical and health consequences of disasters. Background: Almost 24 years ago a major earthquake devastated the northwestern region of Soviet Armenia. The National Aeronautics and Space Administration deployed a telemedicine spacebridge, which operated uninterrupted for 3 months, extending its services to the remote region of Ufa to help the burn victims, mostly children, from a railroad explosion accident. Expert consultations were provided by four major medical center from the United States and several military and civilian medical services of the Soviet Union. Lessons Learned: Disasters continue to contribute to increased morbidity and mortality with significant economic impacts worldwide. Psychological, physical, and social sequelae persist years after the events. Many pre-existing socioeconomic conditions are aggravated following disasters. Telemedicine is a useful medical and public health technology that continues to be underutilized due to the lack of inclusion in the preparedness planning, training, availability of networks, and connectivity costs. Policy Implications: Natural and human-made disasters require both near-term and long-term interventions to reduce morbidity and mortality among the surviving victims. Telemedicine, information technology, and modern portable communication devices should be incorporated in disaster preparedness and recovery training and operations.
C1 [Nicogossian, Arnauld E.] George Mason Univ, Ctr Study Int Med Policies & Practices, Sch Publ Policy, Arlington, VA 22201 USA.
   [Doarn, Charles R.] Univ Cincinnati, Dept Publ Hlth Sci, Cincinnati, OH USA.
   [Doarn, Charles R.] NASA Headquarters, Off Chief Hlth & Med Officer, Washington, DC USA.
RP Nicogossian, AE (reprint author), George Mason Univ, Ctr Study Int Med Policies & Practices, Sch Publ Policy, Founders Hall,Room 549,3351 Fairfax Dr, Arlington, VA 22201 USA.
EM anicogos@gmu.edu
NR 30
TC 3
Z9 3
U1 2
U2 8
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1530-5627
J9 TELEMED E-HEALTH
JI Telemed. e-Health
PD NOV
PY 2011
VL 17
IS 9
BP 741
EP 745
DI 10.1089/tmj.2011.0118
PG 5
WC Health Care Sciences & Services
SC Health Care Sciences & Services
GA 842HT
UT WOS:000296588400013
PM 21861701
ER

PT J
AU DellaCorte, C
AF DellaCorte, Christopher
TI Reflect, remember, celebrate and smile: A tribute to Harold E. Sliney
SO TRIBOLOGY & LUBRICATION TECHNOLOGY
LA English
DT Biographical-Item
C1 NASA, Glenn Res Ctr, Cleveland, OH USA.
RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
EM christopher.dellacorte@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS
PI PARK RIDGE
PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA
SN 1545-858X
J9 TRIBOL LUBR TECHNOL
JI Tribol. Lubr. Technol.
PD NOV
PY 2011
VL 67
IS 11
BP 18
EP 18
PG 1
WC Engineering, Mechanical
SC Engineering
GA 843KT
UT WOS:000296671400007
ER

PT J
AU Shukla, SP
   Chandler, MA
   Rind, D
   Sohl, LE
   Jonas, J
   Lerner, J
AF Shukla, Sonali P.
   Chandler, Mark A.
   Rind, David
   Sohl, Linda E.
   Jonas, Jeff
   Lerner, Jean
TI Teleconnections in a warmer climate: the pliocene perspective
SO CLIMATE DYNAMICS
LA English
DT Article
DE Teleconnections; Pliocene; El Padre; Indian Ocean dipole; El Nino
ID INDIAN-OCEAN DIPOLE; EL-NINO; EXTRATROPICAL RESPONSE; GLACIAL MELTWATER;
   TROPICAL CLIMATE; CIRCULATION; MODEL; ATMOSPHERE; ENSO; PROPAGATION
AB Migrations toward altered sea surface temperature (SST) patterns in the Indo-Pacific region are present in the recent observational record and in future global warming projections. These SSTs are in the form of "permanent" El Nio-like (herein termed "El Padre") and Indian Ocean Dipole (IOD)-like patterns. The Early Pliocene Warm Period, which bears similarity to future warming projections, may have also exhibited these Indo-Pacific SST patterns, as suggested by regional terrestrial paleo-climatic data and general circulation model studies. The ability to corroborate this assessment with paleo-data reconstructions is an advantage of the warm Pliocene period that is not afforded by future warming scenarios. Thus, the Pliocene period provides us with a warm-climate perspective and test bed for understanding potential changes to future atmospheric interactions given these altered SST states. This study specifically assesses how atmospheric teleconnections from El Padre/IOD SST patterns are generated and propagate to create the regional climate signals of the Pliocene period, as these signals may be representative of future regional climatic changes as well. To do this, we construct a holistic diagnostic rubric that allows us to examine atmospheric teleconnections, both energetically and dynamically, as produced by a general circulation model. We incorporate KE', a diagnostic adapted from the eddy kinetic energy generation field, to assess the available energy transferred to these teleconnections. Using this methodology, we found that relative to our Modern Control experiments, weaker atmospheric teleconnections prevail under warm Pliocene conditions, although pathways of propagation still appear directed toward the southwestern United States from our tropical Pacific sector forcing. Propagation directly emanating from the Indian Ocean forcing sector appears to be largely blocked, although indirect teleconnective pathways appear traversing the Asian continent toward the North Pacific. The changes in the atmospheric circulation of Indian Ocean region in response to the underlying specified SST forcing (and indicated by Pliocene paleo-data) may have a host of implications for energy transfer out of and into the region, including interactions with the Asian jet stream and changes to the seasonal monsoon cycle. These interactions warrant further study in both past and future warm climate scenarios.
C1 [Shukla, Sonali P.] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA.
   [Shukla, Sonali P.; Rind, David] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA.
   [Chandler, Mark A.; Sohl, Linda E.; Jonas, Jeff; Lerner, Jean] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP Shukla, SP (reprint author), Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA.
EM sps2113@columbia.edu
FU National Science Foundation [ATM-0323516]; NASA
FX Funding for this research was provided by the National Science
   Foundation, ATM-0323516 (to Chandler), and the NASA Climate Program.
NR 36
TC 4
Z9 4
U1 0
U2 15
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD NOV
PY 2011
VL 37
IS 9-10
BP 1869
EP 1887
DI 10.1007/s00382-010-0976-y
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 840XY
UT WOS:000296476600011
ER

PT J
AU Garrison, JL
   Voo, JK
   Yueh, SH
   Grant, MS
   Fore, AG
   Haase, JS
AF Garrison, James L.
   Voo, Justin K.
   Yueh, Simon H.
   Grant, Michael S.
   Fore, Alexander G.
   Haase, Jennifer S.
TI Estimation of Sea Surface Roughness Effects in Microwave Radiometric
   Measurements of Salinity Using Reflected Global Navigation Satellite
   System Signals
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Bistatic radar; microwave radiometry; ocean salinity; radar remote
   sensing
ID DELAY-DOPPLER MAPS; BRIGHTNESS TEMPERATURE; GPS SIGNALS; WIND-SPEED;
   OCEAN
AB In February-March 2009, an airborne field campaign was conducted using the Passive Active L- and S-band (PALS) microwave sensor and the Ku-band Polarimetric Scatterometer to collect measurements of brightness temperature and near-surface wind speeds. Flights were conducted over a region of expected high-speed winds in the Atlantic Ocean, for the purposes of algorithm development for sea surface salinity (SSS) retrievals. Wind speeds encountered during the March 2, 2009, flight ranged from 5 to 25 m/s. The Global Positioning System (GPS) delay mapping receiver from the National Aeronautics and Space Administration (NASA) Langley Research Center was also flown to collect GPS signals reflected from the ocean surface and generate postcorrelation power-versus-delay measurements. These data were used to estimate ocean surface roughness. These estimates were found to be strongly correlated with PALS-measured brightness temperature. Initial results suggest that reflected GPS measurements made using small low-power instruments can be used to correct the roughness effects in radiometer brightness temperature measurements to retrieve accurate SSS.
C1 [Garrison, James L.; Voo, Justin K.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
   [Yueh, Simon H.; Fore, Alexander G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Grant, Michael S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Haase, Jennifer S.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
RP Garrison, JL (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
EM jgarriso@ecn.purdue.edu; jvoo@purdue.edu; simon.h.yueh@jpl.nasa.gov;
   michael.s.grant@nasa.gov; alexander.fore@jpl.nasa.gov;
   jennifer.s.haase@purdue.edu
FU National Aeronautics and Space Administration (NASA) [NNX08A087G,
   NNX07A049H];  [0802887NSF]
FX Manuscript received January 20, 2011; revised April 11, 2011; accepted
   May 5, 2011. Date of publication July 18, 2011; date of current version
   October 28, 2011. This work was supported by the National Aeronautics
   and Space Administration (NASA) under Grant NNX08A087G, "Comparison of
   GNSS-R Ocean Roughness Measurements with Radiometric and Scattering
   Models at L-band and S-band." The work of J. K. Voo was supported by the
   NASA Earth and Space Science Fellowship Program under Grant NNX07A049H
   to conduct a portion of this work at the Jet Propulsion Laboratory. The
   work of J. S. Haase was supported by Grant 0802887NSF.; The work
   described in this letter that was performed by the Jet Propulsion
   Laboratory, California Institute of Technology, was carried out under a
   contract with the National Aeronautics and Space Administration (NASA).
   The authors would like to thank the P-3 crew of the NASA Wallops Flight
   Facility for their technical expertise and hard work in assisting them
   in conducting this experiment. The authors thank B. Clauss for
   assistance with the data collection.
NR 24
TC 10
Z9 10
U1 1
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD NOV
PY 2011
VL 8
IS 6
BP 1170
EP 1174
DI 10.1109/LGRS.2011.2159323
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA 840SQ
UT WOS:000296462000033
ER

PT J
AU Halekas, JS
   Saito, Y
   Delory, GT
   Farrell, WM
AF Halekas, J. S.
   Saito, Y.
   Delory, G. T.
   Farrell, W. M.
TI New views of the lunar plasma environment
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 1st Workshop on Lunar Dust, Plasma and Atmosphere - The Next Steps
   (LDAP)
CY JAN 27-29, 2010
CL Boulder, CO
SP NASA Lunar Sci Inst (NLSI), Colorado Ctr Lunar Dust & Atmospher Studies (CCLDAS)
DE Moon; Plasma
ID CRUSTAL MAGNETIC-ANOMALIES; SOLAR-WIND INTERACTION; IN-CELL SIMULATIONS;
   UPSTREAM ULF WAVES; HYBRID SIMULATIONS; TERMINATOR REGION; FIELD
   STRUCTURE; CHARGED DUST; MOON; WAKE
AB A rich set of new measurements has greatly expanded our understanding of the Moon-plasma interaction over the last sixteen years, and helped demonstrate the fundamentally kinetic nature of many aspects thereof. Photon and charged particle impacts act to charge the lunar surface, forming thin Debye-scale plasma sheaths above both sunlit and shadowed hemispheres. These impacts also produce photoelectrons and secondary electrons from the surface, as well as ions from the surface and exosphere, all of which in turn feed back into the plasma environment. The solar wind interacts with sub-ion-inertial-scale crustal magnetic fields to form what may be the smallest magnetospheres in the solar system. Proton gyro-motion, solar wind pickup of protons scattered from the dayside surface, and plasma expansion into vacuum each affect the dynamics and structure of different portions of the lunar plasma wake. The Moon provides us with a basic plasma physics laboratory for the study of fundamental processes, some of which we cannot easily observe elsewhere. At the same time, the Moon provides us with a test bed for the study of processes that also operate at many other solar system bodies. We have learned much about the Moon-plasma interaction, with implications for other space and planetary environments. However, many fundamental problems remain unsolved, including the details of the coupling between various parts of the plasma environment, as well as between plasma and the surface, neutral exosphere, and dust. In this paper, we describe our current understanding of the lunar plasma environment, including illustrative new results from Lunar Prospector and Kaguya, and outstanding unsolved problems. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Halekas, J. S.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Saito, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan.
   [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Halekas, J. S.; Delory, G. T.; Farrell, W. M.] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Halekas, JS (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM jazzman@ssl.berkeley.edu
RI Farrell, William/I-4865-2013; 
OI Halekas, Jasper/0000-0001-5258-6128
NR 129
TC 54
Z9 56
U1 0
U2 21
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 NOV
PY 2011
VL 59
IS 14
SI SI
BP 1681
EP 1694
DI 10.1016/j.pss.2010.08.011
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 837GQ
UT WOS:000296179500003
ER

PT J
AU Glenar, DA
   Stubbs, TJ
   McCoy, JE
   Vondrak, RR
AF Glenar, David A.
   Stubbs, Timothy J.
   McCoy, James E.
   Vondrak, Richard R.
TI A reanalysis of the Apollo light scattering observations, and
   implications for lunar exospheric dust
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 1st Workshop on Lunar Dust, Plasma and Atmosphere - The Next Steps
   (LDAP)
CY JAN 27-29, 2010
CL Boulder, CO
SP NASA Lunar Sci Inst (NLSI), Colorado Ctr Lunar Dust & Atmospher Studies (CCLDAS)
DE Moon; Horizon glow; Optical scattering; Lunar dust; Lunar exosphere
ID ZODIACAL LIGHT; PLANETARY SATELLITES; SKY BRIGHTNESS; SOLAR CORONA;
   SPACE; SURFACE; CLOUDS
AB Conspicuous excess brightness, exceeding that expected from coronal and zodiacal light (CZL), was observed above the lunar horizon in the Apollo 15 coronal photographic sequence acquired immediately after orbital sunset (surface sunrise). This excess brightness systematically faded as the Command Module moved farther into shadow, eventually becoming indistinguishable from the CZL background. These observations have previously been attributed to scattering by ultrafine dust grains (radius similar to 0.1 microns) in the lunar exosphere, and used to obtain coarse estimates of dust concentration at several altitudes and an order-of-magnitude estimate of similar to 10(-9) g cm(-2) for the column mass of dust near the terminator, collectively referred to as model "0".
   We have reanalyzed the Apollo 15 orbital sunset sequence by incorporating the known sightline geometries in a Mie-scattering simulation code, and then inverting the measured intensities to retrieve exospheric dust concentration as a function of altitude and distance from the terminator. Results are presented in terms of monodisperse (single grain size) dust distributions. For a grain radius of 0.10 microns, our retrieved dust concentration near the terminator (similar to 0.010 cm(-3)) is in agreement with model "0" at z=10 km, as is the dust column mass (similar to 3-6 x 10(-10) g cm(-2),) but the present results indicate generally larger dust scale heights, and much lower concentrations near 1 km (< 0.08 cm(-3) vs. a few times 0.1 cm(-3) for model "0"). The concentration of dust at high altitudes (z > 50 km) is virtually unconstrained by the measurements. The dust exosphere extends into shadow a distance somewhere between 100 and 200 km from the terminator, depending on the uncertain contribution of CZL to the total brightness. These refined estimates of the distribution and concentration of exospheric dust above the lunar sunrise terminator should place new and more rigorous constraints on exospheric dust transport models, as well as provide valuable support for upcoming missions such as the Lunar Atmosphere and Dust Environment Explorer (LADEE). (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Glenar, David A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
   [Glenar, David A.; Stubbs, Timothy J.; Vondrak, Richard R.] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA USA.
   [Stubbs, Timothy J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
   [Stubbs, Timothy J.; Vondrak, Richard R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [McCoy, James E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Glenar, DA (reprint author), New Mexico State Univ, Dept Astron, POB 30001,MSC 4500, Las Cruces, NM 88003 USA.
EM dglenar@nmsu.edu
RI Stubbs, Timothy/I-5139-2013
OI Stubbs, Timothy/0000-0002-5524-645X
NR 36
TC 25
Z9 25
U1 0
U2 8
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 NOV
PY 2011
VL 59
IS 14
SI SI
BP 1695
EP 1707
DI 10.1016/j.pss.2010.12.003
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 837GQ
UT WOS:000296179500004
ER

PT J
AU Collier, MR
   Hills, HK
   Stubbs, TJ
   Halekas, JS
   Delory, GT
   Espley, J
   Farrell, WM
   Freeman, JW
   Vondrak, R
AF Collier, Michael R.
   Hills, H. Kent
   Stubbs, Timothy J.
   Halekas, Jasper S.
   Delory, Gregory T.
   Espley, Jared
   Farrell, William M.
   Freeman, John W.
   Vondrak, Richard
TI Lunar surface electric potential changes associated with traversals
   through the Earth's foreshock
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 1st Workshop on Lunar Dust, Plasma and Atmosphere - The Next Steps
   (LDAP)
CY JAN 27-29, 2010
CL Boulder, CO
SP NASA Lunar Sci Inst (NLSI), Colorado Ctr Lunar Dust & Atmospher Studies (CCLDAS)
DE Moon; Lunar surface potential; Bow shock; Foreshock; Secondary electron
   emission
ID SOLAR-WIND OBSERVATIONS; BOW SHOCK; PHOTOELECTRON LAYER; TERMINATOR
   REGION; DUST; PLASMA; MOON; EMISSION; SPACE; MAGNETOPAUSE
AB We report an analysis of one year of Suprathermal Ion Detector Experiment (SIDE) Total Ion Detector (TID) "resonance" events observed between January 1972 and January 1973. The study includes only those events during which upstream solar wind conditions were readily available. The analysis shows that these events are associated with lunar traversals through the dawn flank of the terrestrial magnetospheric bow shock. We propose that the events result from an increase in lunar surface electric potential effected by secondary electron emission due to primary electrons in the Earth's foreshock region (although primary ions may play a role as well). This work establishes (1) the lunar surface potential changes as the Moon moves through the terrestrial bow shock, (2) the lunar surface achieves potentials in the upstream foreshock region that differ from those in the downstream magnetosheath region, (3) these differences can be explained by the presence of energetic electron beams in the upstream foreshock region and (4) if this explanation is correct, the location of the Moon with respect to the terrestrial bow shock influences lunar surface potential. Published by Elsevier Ltd.
C1 [Collier, Michael R.; Hills, H. Kent; Stubbs, Timothy J.; Espley, Jared; Farrell, William M.; Vondrak, Richard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Hills, H. Kent] Adnet Syst Inc, Lanham, MD USA.
   [Stubbs, Timothy J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
   [Halekas, Jasper S.; Delory, Gregory T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Freeman, John W.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
   [Collier, Michael R.; Stubbs, Timothy J.; Halekas, Jasper S.; Delory, Gregory T.; Farrell, William M.; Vondrak, Richard] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Collier, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM michael.r.collier@nasa.gov
RI Espley, Jared/I-5118-2013; Collier, Michael/I-4864-2013; Stubbs,
   Timothy/I-5139-2013; Farrell, William/I-4865-2013; 
OI Espley, Jared/0000-0002-6371-9683; Collier, Michael/0000-0001-9658-6605;
   Stubbs, Timothy/0000-0002-5524-645X; Halekas, Jasper/0000-0001-5258-6128
NR 77
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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 NOV
PY 2011
VL 59
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SC Astronomy & Astrophysics
GA 837GQ
UT WOS:000296179500006
ER

PT J
AU Marshall, J
   Richard, A
   Davis, S
AF Marshall, J.
   Richard, A.
   Davis, S.
TI Electrical stress and strain in lunar regolith simulants
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 1st Workshop on Lunar Dust, Plasma and Atmosphere - The Next Steps
   (LDAP)
CY JAN 27-29, 2010
CL Boulder, CO
SP NASA Lunar Sci Inst (NLSI), Colorado Ctr Lunar Dust & Atmospher Studies (CCLDAS)
DE Moon; Dust; Powders; Electrostatics; Griffith flaws; Electrical stress
ID DUST; MOON
AB Experiments to entrain dust with electrostatic and fluid-dynamic forces result in particulate clouds of aggregates rather than individual dust grains. This is explained within the framework of Griffith-flaw theory regarding the comminution/breakage of weak solids. Physical and electrical inhomogeneities in powders are equivalent to microcracks in solids insofar as they facilitate failure at stress risers. Electrical charging of powders induces bulk sample stresses similar to mechanical stresses experienced by strong solids, depending on the nature of the charging. A powder mass therefore "breaks" into clumps rather than separating into individual dust particles. This contrasts with the expectation that electrical forces on the Moon will eject a submicron population of dust from the regolith into the exosphere. A lunar regolith will contain physical and electrostatic inhomogeneities similar to those in most charged powders. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Marshall, J.] SETI Inst, Mountain View, CA 94043 USA.
   [Richard, A.] San Jose State Univ Res Fdn, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Marshall, J (reprint author), SETI Inst, 189 N Bernardo Ave, Mountain View, CA 94043 USA.
EM jmarshall@seti.org; denis.thomas.richard@nasa.gov;
   sanford.s.davis@nasa.gov
NR 18
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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 NOV
PY 2011
VL 59
IS 14
SI SI
BP 1744
EP 1748
DI 10.1016/j.pss.2010.11.005
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 837GQ
UT WOS:000296179500007
ER

PT J
AU Kubrick, RL
   Klaus, DM
   Street, KW
AF Kubrick, Ryan L.
   Klaus, David M.
   Street, Kenneth W., Jr.
TI Defining an abrasion index for lunar surface systems as a function of
   dust interaction modes and variable concentration zones
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 1st Workshop on Lunar Dust, Plasma and Atmosphere - The Next Steps
   (LDAP)
CY JAN 27-29, 2010
CL Boulder, CO
SP NASA Lunar Sci Inst (NLSI), Colorado Ctr Lunar Dust & Atmospher Studies (CCLDAS)
DE Two-body abrasion; Three-body abrasion; Lunar dust; Exploration; Surface
   systems
AB Unexpected issues were encountered during the Apollo era of lunar exploration due to detrimental abrasion of materials upon exposure to the fine-grained, irregular shaped dust on the surface of the Moon. For critical design features involving contact with the lunar surface and for astronaut safety concerns, operational concepts and dust tolerance must be considered in the early phases of mission planning. To systematically define material selection criteria, dust interaction can be characterized by two-body or three-body abrasion testing, and sub-categorically by physical interactions of compression, rolling, sliding, and bending representing specific applications within the system. Two-body abrasion occurs when a single particle or asperity slides across a given surface removing or displacing material. Three-body abrasion occurs when multiple particles interact with a solid surface, or in between two surfaces, allowing the abrasives to freely rotate and interact with the material(s), leading to removal or displacement of mass. Different modes of interaction are described in this paper along with corresponding types of tests that can be utilized to evaluate each configuration. In addition to differential modes of abrasion, variable concentrations of dust in different zones can also be considered for a given system design and operational protocol. These zones include (1) outside the habitat where extensive dust exposure occurs, (2) in a transitional zone such as an airlock or suitport, and (3) inside the habitat or spacesuit with a low particle count. These zones can be used to help define dust interaction frequencies, and corresponding risks to the systems and/or crew can be addressed by appropriate mitigation strategies. An abrasion index is introduced that includes the level of risk, R, the hardness of the mineralogy, H, the severity of the abrasion mode, S. and the frequency of particle interactions, F. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Kubrick, Ryan L.; Klaus, David M.] Univ Colorado, Boulder, CO 80309 USA.
   [Street, Kenneth W., Jr.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Kubrick, RL (reprint author), Univ Colorado, 429 UCB, Boulder, CO 80309 USA.
EM Kobrick@Colorado.edu; Klaus@Colorado.edu; Kenneth.W.Street@nasa.gov
NR 29
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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 NOV
PY 2011
VL 59
IS 14
SI SI
BP 1749
EP 1757
DI 10.1016/j.pss.2010.10.010
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 837GQ
UT WOS:000296179500008
ER

PT J
AU Wang, X
   Horanyi, M
   Robertson, S
AF Wang, X.
   Horanyi, M.
   Robertson, S.
TI Dust transport near electron beam impact and shadow boundaries
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 1st Workshop on Lunar Dust, Plasma and Atmosphere - The Next Steps
   (LDAP)
CY JAN 27-29, 2010
CL Boulder, CO
SP NASA Lunar Sci Inst (NLSI), Colorado Ctr Lunar Dust & Atmospher Studies (CCLDAS)
ID PONDED DEPOSITS; EROS; 433-EROS
AB When the moon enters the plasma sheet of the earth, high energy electron fluxes are incident upon the lunar surface. Some regions are in the shadow of these fluxes due to topographic features. Large electric fields were found at similar shadow boundaries created by the electron beams incident upon an obstacle in the laboratory. Potentials on the beam-illuminated surface follow beam energies and were negative relative to potentials on the shadowed surface. Charged dust particles in the beam-illuminated region were observed to move into the shadow due to these electric fields. The oblique incidence of the electron fluxes upon craters can lead to a portion of the crater surface in the beam-illumination and another portion in the shadow. Dust particles on the slopes of the craters can thus experience large electric fields and transport downhill to fill the bottom of the craters. This mechanism may contribute to the formation of dust ponds observed by the NEAR-Shoemaker spacecraft at Eros, and might be at work on the lunar surface as well. In the laboratory, we used electron fluxes with energies up to 90 eV to bombard an insulating half-pipe. An angle of incidence was chosen so that the impact occurred on farside of the slope and left the bottom and the nearside slope in the shadow. Dust particles on the beam-illuminated slope moved down along the surface toward the bottom of the half-pipe and hopped to the bottom as well, while particles on the shadowed slope remained at rest. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Wang, X.; Horanyi, M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
   [Horanyi, M.; Robertson, S.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
   [Wang, X.; Horanyi, M.; Robertson, S.] NASA, Lunar Sci Inst, CCLDAS, Boulder, CO 80309 USA.
RP Wang, X (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM xu.wang@colorado.edu
OI Horanyi, Mihaly/0000-0002-5920-9226
NR 16
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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 NOV
PY 2011
VL 59
IS 14
SI SI
BP 1791
EP 1794
DI 10.1016/j.pss.2010.12.005
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 837GQ
UT WOS:000296179500012
ER

PT J
AU Pines, V
   Zlatkowski, M
   Chait, A
AF Pines, Vladimir
   Zlatkowski, Marianna
   Chait, Arnon
TI Lofted charged dust distribution above the Moon surface
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 1st Workshop on Lunar Dust, Plasma and Atmosphere - The Next Steps
   (LDAP)
CY JAN 27-29, 2010
CL Boulder, CO
SP NASA Lunar Sci Inst (NLSI), Colorado Ctr Lunar Dust & Atmospher Studies (CCLDAS)
DE Moon environment; Solar wind plasma; Dusty plasma; Plasma sheath
   formation
ID SOLAR-WIND; ION COLLECTION; FLOWING PLASMA; PARTICLES; SPHERE; SHEATH;
   SPACE
AB We developed kinetic theory for the charging processes of small dust grains near the lunar surface due to interaction with the anisotropic solar wind plasma. Once charged, these dust grains, which are exposed to the electric field in the sheath region near the lunar surface, could loft and distribute around such heights off the surface where they reach equilibrium with the local gravitational force. Analytical solutions were derived for the charging time, grain floating potential, and grain charge, characterizing the charging processes of small dust grains in a two-component and in a multi-component solar wind plasma, and further highlighting the unique features presented by the high streaming plasma velocity. We have also formulated a novel kinetic theory of sheath formation around an absorbing planar surface immersed in the anisotropic solar wind plasma in the case of a negligible photoelectric effect and presented solutions for the sheath structure. In this study we combined the results from these analyses and provided estimates for the size distribution function of dust that is expected to be lofted in regions dominated by the solar wind plasma, such as near the terminator and in nearby shadowed craters. Corresponding to the two dominant streaming velocity peaks of 300 and 800 km/s, mean dust diameters of 500 and 350 nm, respectively, are expected to be found at equilibrium at heights of relevance to exploration operations, e.g., around 1.5 m height off the lunar surface. In shadowed craters near the terminator region, where isotropic plasma should be dominating, we estimate mean lofted dust diameter of 800 nm around the same 1.5 m height off the lunar surface. The generally applicable solutions could be used to readily calculate the expected lofted size distribution near the lunar surface as a function of plasma parameters, dust grain composition, and other parameters of interest. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Pines, Vladimir; Zlatkowski, Marianna; Chait, Arnon] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Pines, V (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM vpines@oh.rr.com
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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 NOV
PY 2011
VL 59
IS 14
SI SI
BP 1795
EP 1803
DI 10.1016/j.pss.2011.01.013
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 837GQ
UT WOS:000296179500013
ER

PT J
AU Richard, DT
   Glenar, DA
   Stubbs, TJ
   Davis, SS
   Colaprete, A
AF Richard, D. T.
   Glenar, D. A.
   Stubbs, T. J.
   Davis, S. S.
   Colaprete, A.
TI Light scattering by complex particles in the Moon's exosphere: Toward a
   taxonomy of models for the realistic simulation of the scattering
   behavior of lunar dust
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 1st Workshop on Lunar Dust, Plasma and Atmosphere - The Next Steps
   (LDAP)
CY JAN 27-29, 2010
CL Boulder, CO
SP NASA Lunar Sci Inst (NLSI), Colorado Ctr Lunar Dust & Atmospher Studies (CCLDAS)
DE Moon; Dust; Radiative transfer; Scattering; Polarization
ID DYNAMIC FOUNTAIN MODEL; GRAINS; LEVITATION; SURFACES; SHEATH; SPACE
AB It is suspected that the lunar exosphere has a dusty component dispersed above the surface by various physical mechanisms. Most of the evidence for this phenomenon comes from observations of "lunar horizon glow" (LHG), which is thought to be produced by the scattering of sunlight by this exospheric dust. The characterization of exospheric dust populations at the Moon is key to furthering our understanding of fundamental surface processes, as well as a necessary requirement for the planning of future robotic and human exploration.
   We present a model to simulate the scattering of sunlight by complex lunar dust grains (i.e. grains that are non-spherical and can be inhomogeneous in composition) to be used in the interpretation of remote sensing data from current and future lunar missions. We numerically model lunar dust grains with several different morphologies and compositions and compute their individual scattering signatures using the Discrete Dipole Approximation (DDA). These scattering properties are then used in a radiative transfer code to simulate the light scattering due to a dust size distribution, as would likely be observed in the lunar exosphere at high altitudes 10's of km. We demonstrate the usefulness and relevance of our model by examining mode: irregular grains, aggregate of spherical monomers and spherical grains with nano-phase iron inclusions. We subsequently simulate the scattering by two grain size distributions (0.1 and 0.3 mu m radius), and show the results normalized per-grain. A similar methodology can also be applied to the analysis of the LHG observations, which are believed to be produced by scattering from larger dust grains within about a meter of the surface.
   As expected, significant differences in scattering properties are shown between the analyses employing the widely used Mie theory and our more realistic grain geometries. These differences include large variations in intensity as well as a positive polarization of scattered sunlight caused by non-spherical grains. Positive polarization occurs even when the grain size is small compared to the wavelength of incident sunlight, thus confirming that the interpretation of LHG based on Mie theory could lead to large errors in estimating the distribution and abundances of exospheric dust. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Richard, D. T.; Davis, S. S.; Colaprete, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Richard, D. T.] San Jose State Univ Res Fdn, San Jose, CA USA.
   [Glenar, D. A.] New Mexico State Univ, Las Cruces, NM 88003 USA.
   [Stubbs, T. J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
   [Stubbs, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Richard, D. T.; Glenar, D. A.; Stubbs, T. J.; Davis, S. S.; Colaprete, A.] NASA, Lunar Sci Inst, Moffett Field, CA USA.
RP Richard, DT (reprint author), NASA, Ames Res Ctr, Bldg N245,Room 301,Mail Stop 245-3, Moffett Field, CA 94035 USA.
EM denis.thomas.richard@nasa.gov
RI Stubbs, Timothy/I-5139-2013
OI Stubbs, Timothy/0000-0002-5524-645X
NR 46
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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 NOV
PY 2011
VL 59
IS 14
SI SI
BP 1804
EP 1814
DI 10.1016/j.pss.2011.01.003
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 837GQ
UT WOS:000296179500014
ER

PT J
AU Jiao, LG
   Kuang, WJ
   Ma, SZ
AF Jiao LiGuo
   Kuang WeiJia
   Ma ShiZhuang
TI Numerical simulations on origin of Galilean moons' magnetic anomalies
SO SCIENCE CHINA-EARTH SCIENCES
LA English
DT Article
DE Galilean moons; magnetic fields; magneto-convection; dynamo
ID SUBSURFACE OCEANS; DYNAMO ACTION; FIELD; EUROPA; CALLISTO; GANYMEDE;
   PLASMA; STATE; CORE
AB Galileo mission detected the magnetic anomalies originated from Galilean moons. These anomalies are likely generated in the moons' interiors, under the influence of a strong ambient Jovian field. Among various possible generation mechanisms of the anomalies, we focus on magneto-convection and dynamos in the interiors via numerical simulation. To mimic the electromagnetic environment of the moons, we introduce in our numerical model an external uniform magnetic field B (0) with a fixed orientation but varying field strength. Our results show that a finite B (0) can substantially alter the dynamo processes inside the core. When the ambient field strength B (0) increases to approximately 40% of the field generated by the pure dynamo action, the convective state in the core changes significantly: the convective flow decreases by 80% in magnitude, but the differential rotation becomes stronger in much of the fluid layer, leading to a stronger field generated in the core. The field morphologies inside the core tend to align with the ambient field, while the flow patterns show the symmetry-breaking effect under the influence of B (0). Furthermore, the generated field tends to be temporally more stable.
C1 [Jiao LiGuo; Ma ShiZhuang] Chinese Acad Sci, Grad Univ, Coll Earth Sci, Lab Computat Geodynam, Beijing 100049, Peoples R China.
   [Kuang WeiJia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Jiao, LG (reprint author), Chinese Acad Sci, Grad Univ, Coll Earth Sci, Lab Computat Geodynam, Beijing 100049, Peoples R China.
EM liguo1978.jiao@gmail.com
RI Kuang, Weijia/K-5141-2012
OI Kuang, Weijia/0000-0001-7786-6425
FU National Natural Science Foundation of China [40328006]; NASA
FX We thank Drs. Jiang Weiyuan, Wei Zigang, Zhou Yuanze, Warner Juying and
   Xu Wenyao for providing various help through this work. This work was
   supported by National Natural Science Foundation of China (Grant No.
   40328006). Kuang Weijia was also supported by MFRP and ESIP from NASA.
NR 25
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PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 1674-7313
J9 SCI CHINA EARTH SCI
JI Sci. China-Earth Sci.
PD NOV
PY 2011
VL 54
IS 11
BP 1754
EP 1760
DI 10.1007/s11430-011-4276-0
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 839OW
UT WOS:000296378400012
ER

PT J
AU Arkoosh, MR
   Strickland, S
   Van Gaest, A
   Ylitalo, GM
   Johnson, L
   Yanagida, GK
   Collier, TK
   Dietrich, JP
AF Arkoosh, Mary R.
   Strickland, Stacy
   Van Gaest, Ahna
   Ylitalo, Gina M.
   Johnson, Lyndal
   Yanagida, Gladys K.
   Collier, Tracy K.
   Dietrich, Joseph P.
TI Trends in organic pollutants and lipids in juvenile Snake River spring
   Chinook salmon with different outmigrating histories through the Lower
   Snake and Middle Columbia Rivers
SO SCIENCE OF THE TOTAL ENVIRONMENT
LA English
DT Article
DE Federal Columbia River Power System; Chinook; Lipids; Contaminants;
   Persistent organic pollutants (PCBs and DDTs); PAHs
ID POLYCYCLIC AROMATIC-HYDROCARBONS; TROUT ONCORHYNCHUS-MYKISS;
   RAINBOW-TROUT; ENVIRONMENTAL CONTAMINANTS; POLYCHLORINATED-BIPHENYLS;
   EXPOSURE; FISH; TSHAWYTSCHA; RESPONSES; TOXICITY
AB A three-year field study was conducted from 2006 to 2008 to monitor the spatial and temporal trends of organic pollutants in migrating juvenile Snake River spring Chinook salmon (Oncorhynchus tshawytscha) sampled from the Lower Snake and Middle Columbia River Basins. Specifically, hatchery-reared juvenile salmon were monitored as they navigated the Federal Columbia River Power System (FCRPS) by either transport barge (Barged) or remained in the river (In-River) from Lower Granite Dam to a terminal collection dam, either John Day Dam or Bonneville Dam. Levels of polychlorinated biphenyls (PCBs), polybrominated diphenyl ethers (PBDEs), and organochlorine (OC) pesticides were detected in the bodies of both In-River and Barged salmon during the 2006, 2007 and 2008 outmigrating season. At the terminal dam, In-River fish had greater concentrations of persistent organic pollutants POPs than Barged salmon. Of the POPs detected, dichlorodiphenyltrichloroethanes (DDTs) were found at the greatest concentrations in the salmon bodies. These elevated lipid-normalized concentrations in the In-River fish were due to lipid depletion in all years as well as increased exposure to POPs in some years as indicated by an increase in wet weight contaminant concentrations. Salmon were also exposed to polycyclic aromatic hydrocarbons (PAHs) as indicated by the phenanthrene (PHN) signal for biliary fluorescent aromatic compounds (FACs) at the hatcheries or prior to Lower Granite Dam. There were detectable levels of biliary FACs as fish migrated downstream or were barged to the terminal dam. Therefore, the potential exists for these organic pollutants and lipid levels to cause adverse effects and should be included as one of the variables to consider when examining the effects of the FCRPS on threatened and endangered juvenile salmon. Published by Elsevier B.V.
C1 [Arkoosh, Mary R.; Strickland, Stacy; Van Gaest, Ahna; Dietrich, Joseph P.] Natl Ocean & Atmospher Adm, Environm Conservat Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
   [Ylitalo, Gina M.; Johnson, Lyndal; Yanagida, Gladys K.] NOAA, Environm Conservat Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98112 USA.
   [Collier, Tracy K.] NOAA, Silver Spring, MD 20910 USA.
RP Arkoosh, MR (reprint author), Newport Res Stn, 2032 SE OSU Dr, Newport, OR 97365 USA.
EM mary.arkoosh@noaa.gov
FU US Army Corps of Engineers; NOAA; Northwest Fisheries Science Center's
   Fish Ecology Division
FX Funding for this study was provided, in part, by the Anadromous Fish
   Evaluation Program of the US Army Corps of Engineers and from NOAA
   Fisheries programmatic support for salmon recovery science. We
   appreciate the support of John W. Ferguson, Director of Northwest
   Fisheries Science Center's Fish Ecology Division in helping to obtain
   financial support for this work. We greatly appreciate the technical
   assistance of Jerry Pruiett, Samantha Bund, Paul Peterson, James Lathe,
   Bill Fleenor, Greg Hutchinson, Erik Loboschefsky, Nancy Raskauskas,
   Amber Roegner, Dina Spangenberg, Mary Bhuthimethee, Collin Christianson,
   Ben Campbell, Claudia Bravo, Don Thompson, Kai Eder, and Frank Loge in
   sample collection and care; as well as Jennie Bolton, Daryle Boyd,
   Richard Boyer, Catherine Sloan, and Karen Tilbury in sample and data
   analysis. We thank Paul Olson and Mark Myers for reviewing the
   manuscript.
NR 53
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0048-9697
J9 SCI TOTAL ENVIRON
JI Sci. Total Environ.
PD NOV 1
PY 2011
VL 409
IS 23
BP 5086
EP 5100
DI 10.1016/j.scitotenv.2011.08.031
PG 15
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 836RL
UT WOS:000296128700024
PM 21937091
ER

PT J
AU Doarn, CR
AF Doarn, Charles R.
TI Medical Policy Development for Human Spaceflight at NASA: An Evolution
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE Spaceflight; medical policy; history; space medicine
ID SPACE-MEDICINE
AB DOARN CR. Medical policy development for human spaceflight at NASA: an evolution. Aviat Space Environ Med 2011; 82:1073-7.
   Codification of medical policy for the National Aeronautics and Space Administration (NASA) did not occur until 1977. Policy development was based on NASA's human spaceflight efforts from 1958, and the need to support the operational aspects of the upcoming Space Shuttle Program as well as other future activities. In 1958, the Space Task Group (STG), a part of the National Advisory Committee on Aeronautics (NACA), became the focal point for astronaut selection, medical support, and instrumentation development in support of Project Mercury. NACA transitioned into NASA in 1958. The SIC moved to Houston, TX, in 1961 and became the Manned Spacecraft Center. During these early years, medical support for astronaut selection and healthcare was provided through arrangements with the U.S. military, specifically the United States Air Force, which had the largest group of subject matter experts in aerospace medicine. Through most of the 1960s, the military worked very closely with NASA in developing the foundations of bioastronautics and space medicine. This work was complemented by select individuals from outside the government. From 1958 to 1977, there was no standard approach to medical policy formulation within NASA. During this time, it was individualized and subjected to political pressures. This manuscript documents the evolution of medical policy in the NASA, and provides a historical account of the individuals, processes, and needs to develop policy.
C1 [Doarn, Charles R.] Univ Cincinnati, Dept Publ Hlth Sci, Telemed Program, Cincinnati, OH 45267 USA.
   [Doarn, Charles R.] NASA Headquarters, Off Chief Hlth & Med Officer, Washington, DC USA.
RP Doarn, CR (reprint author), Univ Cincinnati, Dept Publ Hlth Sci, Telemed Program, 260 Stetson,Suite 4200,POB 670840, Cincinnati, OH 45267 USA.
EM charles.doarn@uc.edu
NR 15
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U2 6
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD NOV
PY 2011
VL 82
IS 11
BP 1073
EP 1077
DI 10.3357/ASEM.3103.2011
PG 5
WC Public, Environmental & Occupational Health; Medicine, General &
   Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
   Medicine; Sport Sciences
GA 837DZ
UT WOS:000296172600012
PM 22097646
ER

PT J
AU Jones, B
   Beylkin, G
   Born, G
   Provence, R
AF Jones, Brandon A.
   Beylkin, Gregory
   Born, George H.
   Provence, Robert S.
TI A multiresolution model for small-body gravity estimation
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Gravity modeling; Spherical harmonics; Gravity estimation; Quadratures
   for the sphere; Multiresolution representations; Asteroid Eros
ID MISSION; SPHERE
AB A new model, dubbed the MRQSphere, provides a multiresolution representation of the gravity field designed for its estimation. The multiresolution representation uses an approximation via Gaussians of the solution of the Laplace's equation in the exterior of a sphere. Also, instead of the spherical harmonics, variations in the angular variables are modeled by a set of functions constructed using quadratures for the sphere invariant under the icosahedral group. When combined, these tools specify the spatial resolution of the gravity field as a function of altitude and required accuracy. We define this model, and apply it to representing and estimating the gravity field of the asteroid 433 Eros. We verified that a MRQSphere model derived directly from the true spherical harmonics gravity model satisfies the user defined precision. We also use the MRQSphere model to estimate the gravity field of Eros for a simulated satellite mission, yielding a solution with accuracy only limited by measurement errors and their spatial distribution.
C1 [Jones, Brandon A.; Born, George H.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
   [Beylkin, Gregory] Univ Colorado, Dept Appl Math, Boulder, CO 80309 USA.
   [Provence, Robert S.] NASA, Aerosci & Flight Mech Div, Johnson Space Ctr, Houston, TX 77058 USA.
RP Jones, B (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, UCB 431, Boulder, CO 80309 USA.
EM jonesba@colorado.edu
RI Beylkin, Gregory/G-6653-2011; 
OI BEYLKIN, GREGORY/0000-0003-3447-1460
FU NASA from the Johnson Space Center; AFOSR [FA-9550-07-1-0135]
FX A large portion of this work was funded by a NASA Graduate Student
   Researchers Program (GSRP) fellowship from the Johnson Space Center.
   Gregory Beylkin's work was funded by AFOSR grant FA-9550-07-1-0135. The
   authors would like to thank Cory Ahrens (currently at the Tech-X
   Corporation) for providing the quadratures for this study.
NR 22
TC 2
Z9 2
U1 1
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD NOV
PY 2011
VL 111
IS 3
BP 309
EP 335
DI 10.1007/s10569-011-9374-y
PG 27
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA 836DP
UT WOS:000296089700002
ER

PT J
AU Nikolaev, P
   Menamparambath, MM
   Boul, PJ
   Moloney, P
   Arepalli, S
AF Nikolaev, Pavel
   Menamparambath, Mini Mol
   Boul, Peter J.
   Moloney, Padraig
   Arepalli, Sivaram
TI Raman probing of adhesion loss in carbon nanotube - reinforced composite
SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING
LA English
DT Article
DE Nano-structures; Adhesion
ID EPOXY/SWNT COMPOSITES; MECHANICAL-PROPERTIES; STRAIN; SPECTROSCOPY;
   DEFORMATION; ELASTICITY; STRENGTH; FIBERS; LOAD
AB Raman spectroscopy of a carbon nanotube - reinforced phenolic resin is used to study the interaction of nanotubes with a host matrix. The observed sublinear dependence of the Raman G-band shift on the matrix strain, accompanied by inhomogeneous broadening of the spectral line, is interpreted as a gradual loss of adhesion between nanotubes and the polymer. An approach to simulate the ensemble-averaged Raman response of the nanotubes in composite is proposed, that takes into account nanotube orientation, angular dependence of the polarized Raman response of nanotubes, and adhesion loss between the nanotubes and the polymer. The comparison of the observed Raman line shapes and Raman shifts with simulation provides interesting insights into the micromechanics of nanotube interaction with polymer. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Nikolaev, Pavel; Menamparambath, Mini Mol; Arepalli, Sivaram] Sungkyunkwan Univ, Dept Energy Sci, Suwon 440746, South Korea.
   [Boul, Peter J.] NASA, ERC Inc, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
   [Moloney, Padraig] Rice Univ, Dept Mech Engn & Mat Sci, Houston, TX 77251 USA.
RP Nikolaev, P (reprint author), Sungkyunkwan Univ, Dept Energy Sci, 300 Cheoncheon Dong, Suwon 440746, South Korea.
EM pasha.nikolaev@gmail.com
RI Nikolaev, Pavel/B-9960-2009
FU NRF of Korea [R31-2008-10029, 2010-0006410]; NASA [NNJ05HI05C]
FX This research was supported by WCU program through the NRF of Korea,
   R31-2008-10029, NRF of Korea Grant 2010-0006410, and by NASA under
   Contract # NNJ05HI05C.
NR 35
TC 3
Z9 4
U1 1
U2 17
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1359-835X
J9 COMPOS PART A-APPL S
JI Compos. Pt. A-Appl. Sci. Manuf.
PD NOV
PY 2011
VL 42
IS 11
BP 1681
EP 1686
DI 10.1016/j.compositesa.2011.07.022
PG 6
WC Engineering, Manufacturing; Materials Science, Composites
SC Engineering; Materials Science
GA 837BY
UT WOS:000296167300013
ER

PT J
AU Tapiador, FJ
   Hou, AY
   de Castro, M
   Checa, R
   Cuartero, F
   Barros, AP
AF Tapiador, Francisco J.
   Hou, Arthur Y.
   de Castro, Manuel
   Checa, Ramiro
   Cuartero, Fernando
   Barros, Ana P.
TI Precipitation estimates for hydroelectricity
SO ENERGY & ENVIRONMENTAL SCIENCE
LA English
DT Article
ID RADAR-RAINFALL UNCERTAINTIES; CLIMATE SYSTEM PREDICTION; UNIFIED
   MODELING APPROACH; DROP SIZE DISTRIBUTION; SATELLITE DATA; GAUGE
   MEASUREMENTS; PASSIVE MICROWAVE; SCALE DEPENDENCE; CHANGE IMPACTS;
   HYDROPOWER
AB Hydroelectric plants require precise and timely estimates of rain, snow and other hydrometeors for operations. However, it is far from being a trivial task to measure and predict precipitation. This paper presents the linkages between precipitation science and hydroelectricity, and in doing so it provides insight into current research directions that are relevant for this renewable energy. Methods described include radars, disdrometers, satellites and numerical models. Two recent advances that have the potential of being highly beneficial for hydropower operations are featured: the Global Precipitation Measuring (GPM) mission, which represents an important leap forward in precipitation observations from space, and high performance computing (HPC) and grid technology, that allows building ensembles of numerical weather and climate models.
C1 [Tapiador, Francisco J.; de Castro, Manuel; Checa, Ramiro] UCLM, Inst Environm Sci, Fac Environm Sci & Biochem, Toledo, Spain.
   [Hou, Arthur Y.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
   [Cuartero, Fernando] UCLM, Dept Comp Syst, Albacete, Spain.
   [Barros, Ana P.] Duke Univ, Pratt Sch Engn, Durham, NC 27706 USA.
RP Tapiador, FJ (reprint author), UCLM, Inst Environm Sci, Fac Environm Sci & Biochem, Toledo, Spain.
EM francisco.tapiador@uclm.es
RI Hou, Arthur/D-8578-2012; Barros, Ana/A-3562-2011; Checa-Garcia,
   Ramiro/P-3426-2014
OI Barros, Ana/0000-0003-4606-3106; Checa-Garcia,
   Ramiro/0000-0001-7653-3653
FU MICCIN [CGL2010-20787-C02-01, CGL2010-20787-C02-02]; CENIT PROMETEO;
   JCCM [PPII10-0162-554]; Duke University
FX Support from projects CGL2010-20787-C02-01, CGL2010-20787-C02-02
   (MICCIN), CENIT PROMETEO, and PPII10-0162-554 (JCCM) is acknowledged. A.
   Barros also acknowledges support from ongoing NASA-PMM and NOAASARP
   grants at Duke University.
NR 117
TC 7
Z9 7
U1 3
U2 17
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
   ENGLAND
SN 1754-5692
J9 ENERG ENVIRON SCI
JI Energy Environ. Sci.
PD NOV
PY 2011
VL 4
IS 11
BP 4435
EP 4448
DI 10.1039/c1ee01745d
PG 14
WC Chemistry, Multidisciplinary; Energy & Fuels; Engineering, Chemical;
   Environmental Sciences
SC Chemistry; Energy & Fuels; Engineering; Environmental Sciences & Ecology
GA 837YE
UT WOS:000296248100005
ER

PT J
AU Clune, TL
   Rood, RB
AF Clune, Thomas L.
   Rood, Richard B.
TI Software Testing and Verification in Climate Model Development
SO IEEE SOFTWARE
LA English
DT Editorial Material
ID SIMULATIONS
C1 [Clune, Thomas L.] NASA, Goddard Space Flight Ctr, Adv Software Technol Grp, Div Earth Sci, Greenbelt, MD 20771 USA.
   [Rood, Richard B.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
   [Rood, Richard B.] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA.
RP Clune, TL (reprint author), NASA, Goddard Space Flight Ctr, Adv Software Technol Grp, Div Earth Sci, Greenbelt, MD 20771 USA.
EM thomas.l.clune@nasa.gov; rbrood@umich.edu
RI Rood, Richard/C-5611-2008
OI Rood, Richard/0000-0002-2310-4262
NR 16
TC 6
Z9 6
U1 0
U2 4
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0740-7459
J9 IEEE SOFTWARE
JI IEEE Softw.
PD NOV-DEC
PY 2011
VL 28
IS 6
BP 49
EP 55
DI 10.1109/MS.2011.117
PG 7
WC Computer Science, Software Engineering
SC Computer Science
GA 836HP
UT WOS:000296102300011
ER

PT J
AU Hada, M
   Huff, JL
   Patel, ZS
   Kawata, T
   Pluth, JM
   George, KA
   Cucinotta, FA
AF Hada, Megumi
   Huff, Janice L.
   Patel, Zarana S.
   Kawata, Tetsuya
   Pluth, Janice M.
   George, Kerry A.
   Cucinotta, Francis A.
TI AT cells are not radiosensitive for simple chromosomal exchanges at low
   dose
SO MUTATION RESEARCH-FUNDAMENTAL AND MOLECULAR MECHANISMS OF MUTAGENESIS
LA English
DT Article
DE AT; NBS; Chromosomal aberrations; Radiation sensitivity; DSB repair
ID DOUBLE-STRAND BREAKS; IN-SITU HYBRIDIZATION; ATAXIA-TELANGIECTASIA
   FIBROBLASTS; POTENTIALLY LETHAL DAMAGE; DNA-DAMAGE; RATE IRRADIATION;
   GAMMA-H2AX FOCI; ATM ACTIVATION; REPAIR; ABERRATIONS
AB Cells deficient in ATM (product of the gene that is mutated in ataxia telangiectasia patients) or NBS (product of the gene mutated in the Nijmegen breakage syndrome) show increased yields of both simple and complex chromosomal aberrations after high doses (>0.5 Gy) of ionizing radiation (X-rays or gamma-rays), however less is known on how these cells respond at low dose. Previously we had shown that the increased chromosome aberrations in ATM and NBS defective lines was due to a significantly larger quadratic dose-response term compared to normal fibroblasts for both simple and complex exchanges. The linear dose-response term for simple exchanges was significantly higher in NBS cells compared to wild type cells, but not for AT cells. However, AT cells have a high background level of exchanges compared to wild type or NBS cells that confounds the understanding of low dose responses. To understand the sensitivity differences for high to low doses, chromosomal aberration analysis was first performed at low dose-rates (0.5 Gy/d), and results provided further evidence for the lack of sensitivity for exchanges in AT cells below doses of 1 Gy. Normal lung fibroblast cells treated with KU-55933, a specific ATM kinase inhibitor, showed increased numbers of exchanges at a dose of 1 Gy and higher, but were similar to wild type cells at 0.5 Gy or below. These results were confirmed using siRNA knockdown of ATM. The present study provides evidence that the increased radiation sensitivity of AT cells for chromosomal exchanges found at high dose does not occur at low dose. Published by Elsevier B.V.
C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
   [Hada, Megumi; Huff, Janice L.; Patel, Zarana S.] USRA Div Life Sci, Houston, TX 77058 USA.
   [Kawata, Tetsuya] Keio Univ, Sch Med, Dept Radiol, Tokyo, Japan.
   [Pluth, Janice M.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Life Sci, Berkeley, CA 94720 USA.
   [George, Kerry A.] Wyle, Houston, TX 77058 USA.
RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM Francis.A.Cucinotta@nasa.gov
FU US DOE [DE-A103-05ER64088]; NASA
FX We gratefully acknowledge partial financial support provided by the US
   DOE (DE-A103-05ER64088), and the NASA Space Radiation Program.
NR 37
TC 6
Z9 6
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0027-5107
J9 MUTAT RES-FUND MOL M
JI Mutat. Res.-Fundam. Mol. Mech. Mutagen.
PD NOV 1
PY 2011
VL 716
IS 1-2
BP 76
EP 83
DI 10.1016/j.mrfmmm.2011.08.006
PG 8
WC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
SC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
GA 837FW
UT WOS:000296177500010
PM 21889946
ER

PT J
AU Sabra, MS
   Clemens, MA
   Weller, RA
   Mendenhall, MN
   Barghouty, AF
   Malik, FB
AF Sabra, M. S.
   Clemens, M. A.
   Weller, R. A.
   Mendenhall, M. N.
   Barghouty, A. F.
   Malik, F. B.
TI Validation of nuclear reaction models of 180 MeV proton-induced
   fragmentation of Al-27
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
   INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article
DE Nuclear fragmentation; Cross sections; Monte Carlo simulations
ID EFFECTS RATE PREDICTION; STATISTICAL-MODEL; CROSS-SECTIONS; ENERGY;
   CASCADE
AB Kinetic energy, angular distribution, and isobaric cross section data for A = 7-25 fragments formed in p + Al-27 reaction at bombarding energy of 180 MeV are compared with the calculations of the Binary Cascade Model (BIC), the Cascade Exciton Model (CEM), JQMD/PHITS, as well as the Statistical Model with Final State Interaction (SMESI). For completeness, the kinetic energy spectra of light particles (n, p, alpha) formed in p + Al-27 reaction at bombarding energy of 156 MeV are also presented. A general agreement between the data and predictions of these models is found. However, disagreement with the data for the yields of light-mass fragments as well as near-target fragments is also found and discussed. The importance of this comparative study to simulation and analysis of radiation effects on microscopic electrical components operating in space is also discussed. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Sabra, M. S.; Weller, R. A.; Mendenhall, M. N.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37212 USA.
   [Clemens, M. A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
   [Barghouty, A. F.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
   [Malik, F. B.] So Illinois Univ, Dept Phys, Carbondale, IL 62901 USA.
   [Malik, F. B.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
RP Sabra, MS (reprint author), Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37212 USA.
EM m.sabra@vanderbilt.edu
FU NASA; Defense Thread Reduction Agency
FX This work has been supported by the NASA Advanced Avionics and Processor
   Systems (AAPS) Program and by the Defense Thread Reduction Agency Basic
   Research Program.
NR 36
TC 2
Z9 2
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD NOV 1
PY 2011
VL 269
IS 21
BP 2463
EP 2468
DI 10.1016/j.nimb.2011.07.098
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
   Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 836AO
UT WOS:000296078600001
ER

PT J
AU Badavi, FF
AF Badavi, Francis F.
TI A low earth orbit dynamic model for the proton anisotropy validation
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
   INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article
DE Proton; Anisotropy; LEO; GEORAD; CEASE/TSX-5
ID TRAPPED PROTONS; FLUX
AB Ionizing radiation measurements at low earth orbit (LEO) form the ideal tool for the experimental validation of radiation environmental models, nuclear transport code algorithms and nuclear reaction cross sections. Indeed, prior measurements on the space transportation system (STS; shuttle) have provided vital information impacting both the environmental models and the nuclear transport code development by requiring dynamic models of the LEO environment. Previous studies using computer aided design (CAD) models of the international space station (ISS) have demonstrated that the dosimetric prediction for a spacecraft at LEO requires the description of an environmental model with accurate anisotropic as well as dynamic behavior. This paper describes such a model for the trapped proton. The described model is a component of a suite of codes collectively named GEORAD (GEOmagnetic RADiation) which computes cutoff rigidity, trapped proton and trapped electron environments. The web version of GEORAD is named OLTARIS (On-line Tool for the Assessment of Radiation in Space). GEORAD suite is applicable to radiation environment prediction at LEO, medium earth orbit (MEO) and geosynchronous earth orbit (CEO) at quiet solar periods. GEORAD interest is in the study of long term effect of the trapped environment and therefore it does not account for any short term external field contribution due to solar activity. With the concentration of the paper on the LEO protons only, the paper presents the validation of the trapped proton model within GEORAD with reported measurements from the compact environment anomaly sensor (CEASE) science instrument package, flown onboard the tri-service experiment-5 (TSX-5) satellite during the period of June 2000 to July 2006. The spin stabilized satellite was flown in a 410 x 1710 km, 690 inclination elliptical orbit, allowing it to be exposed to a broad range of the LEO regime. The paper puts particular emphasize on the validation of the differential at 40 MeV, and integral at >40 MeV proton flux profiles, in the vicinity of the south Atlantic anomaly (SAA) region where protons exhibit east-west (EW) anisotropy and have a relatively narrow pitch angle distribution. Within SAA, the EW anisotropy results in different level of exposure to different sections of a formation flying spacecraft such as TSX-5 or ISS. While the magnitude of the EW effect at LEO depends on a multitude of factors such as trapped proton energy, orientation of the spacecraft along the velocity vector and altitude of the spacecraft, the paper draws quantitative conclusions on the combined effect of proton pitch angle and EW anomaly. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Badavi, Francis F.] Christopher Newport Univ, OSP, Newport News, VA 23606 USA.
RP Badavi, FF (reprint author), NASA, Langley Res Ctr, MS 188E, Hampton, VA 23681 USA.
EM francis.f.badavi@nasa.gov
NR 29
TC 1
Z9 2
U1 1
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD NOV 1
PY 2011
VL 269
IS 21
BP 2614
EP 2622
DI 10.1016/j.nimb.2011.08.002
PG 9
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
   Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 836AO
UT WOS:000296078600023
ER

PT J
AU Hemmati, H
   Biswas, A
   Djordjevic, IB
AF Hemmati, Hamid
   Biswas, Abhijit
   Djordjevic, Ivan B.
TI Deep-Space Optical Communications: Future Perspectives and Applications
SO PROCEEDINGS OF THE IEEE
LA English
DT Article
DE Deep-space optical communications; laser communications; lasers;
   photon-counting detectors
ID IN-ORBIT TEST; AVALANCHE PHOTODIODES; DEMONSTRATION MLCD; FIBER LASER;
   SYSTEM; POWER; YAG; ND
AB The concept of deep-space optical communications was formulated shortly after the invention of lasers. The promise of laser communications, high data rate delivery with significantly reduced aperture size for the flight terminal, led to the pursuit of several successful experiments from Earth orbit and provided the incentive for further demonstrations to extend the range to deep space. This paper is aimed at presenting an overview of the current status of optical communications with an emphasis on deep space. Future perspectives and applications of optical communications related to near-Earth and interplanetary communications are also addressed.
C1 [Hemmati, Hamid; Biswas, Abhijit] CALTECH, Jet Prop Lab, Opt Commun Grp, Pasadena, CA 91109 USA.
   [Djordjevic, Ivan B.] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA.
RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, Opt Commun Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM hhemmati@jpl.nasa.gov; abiswas@jpl.nasa.gov; ivan@ece.arizona.edu
FU National Science Foundation (NSF) [CCF-0952711, ECCS-0725405]
FX Manuscript received October 21, 2010; revised April 27, 2011; accepted
   June 18, 2011. Date of publication August 15, 2011; date of current
   version October 19, 2011. 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. It was also supported in part by the National Science
   Foundation (NSF) under Grants CCF-0952711 and ECCS-0725405.
NR 82
TC 23
Z9 23
U1 2
U2 18
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9219
J9 P IEEE
JI Proc. IEEE
PD NOV
PY 2011
VL 99
IS 11
SI SI
BP 2020
EP 2039
DI 10.1109/JPROC.2011.2160609
PG 20
WC Engineering, Electrical & Electronic
SC Engineering
GA 835EE
UT WOS:000296016800014
ER

PT J
AU Atli, KC
   Karaman, I
   Noebe, RD
AF Atli, K. C.
   Karaman, I.
   Noebe, R. D.
TI Work output of the two-way shape memory effect in Ti50.5Ni24.5Pd25
   high-temperature shape memory alloy
SO SCRIPTA MATERIALIA
LA English
DT Article
DE TiNiPd; High-temperature shape memory alloy; Training; Two-way shape
   memory effect; Work output
ID STRESS; LOAD
AB A significant two-way shape memory effect (TWSME) was demonstrated, for the first time, in a TiNiPd high-temperature shape memory alloy (SMA) with TWSM strains as high as 2.6%. This TWSME was able to perform mechanical work, with a maximum work output of 0.12 J g(-1), well above the levels obtained from conventional SMAs. Microstructural changes obtained through severe plastic deformation processing did not improve the TWSME stability and resulted in a reduction of strain capability and work output. (C) 2011 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Atli, K. C.; Karaman, I.] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
   [Karaman, I.] Texas A&M Univ, Mat Sci & Engn Grad Program, College Stn, TX 77843 USA.
   [Noebe, R. D.] NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
RP Karaman, I (reprint author), Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
EM ikaraman@tamu.edu
RI Atli, Kadri/D-6978-2013; Karaman, Ibrahim/E-7450-2010
OI Atli, Kadri/0000-0002-4807-2113; Karaman, Ibrahim/0000-0001-6461-4958
FU NASA; Subsonic Fixed Wing Project [NNX07A-B56A]; Supersonics Project
FX This work was supported by the NASA Fundamental Aeronautics Program,
   Subsonic Fixed Wing Project through Cooperative Agreement No.
   NNX07A-B56A, and the Supersonics Project.
NR 15
TC 16
Z9 17
U1 3
U2 19
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6462
J9 SCRIPTA MATER
JI Scr. Mater.
PD NOV
PY 2011
VL 65
IS 10
BP 903
EP 906
DI 10.1016/j.scriptamat.2011.08.006
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
   Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
   Metallurgical Engineering
GA 834ZL
UT WOS:000296002900014
ER

PT J
AU Heintzenberg, J
   Hermann, M
   Weigelt, A
   Clarke, A
   Kapustin, V
   Anderson, B
   Thornhill, K
   Van Velthoven, P
   Zahn, A
   Brenninkmeijer, C
AF Heintzenberg, Jost
   Hermann, Markus
   Weigelt, Andreas
   Clarke, Antony
   Kapustin, Vladimir
   Anderson, Bruce
   Thornhill, Kenneth
   Van Velthoven, Peter
   Zahn, Andreas
   Brenninkmeijer, Carl
TI Near-global aerosol mapping in the upper troposphere and lowermost
   stratosphere with data from the CARIBIC project
SO TELLUS SERIES B-CHEMICAL AND PHYSICAL METEOROLOGY
LA English
DT Article
ID PARTICLE-PRODUCTION; TROPOPAUSE REGION; CIVIL AIRCRAFT; TRACE GASES;
   DISTRIBUTIONS; VARIABILITY; ATMOSPHERE; EFFICIENCY; EVOLUTION; SYSTEM
AB This study extrapolates aerosol data of the CARIBIC project from 1997 until June 2008 in along trajectories to compose large-scale maps and vertical profiles of submicrometre particle concentrations in the upper troposphere and lowermost stratosphere (UT/LMS). The extrapolation was validated by comparing extrapolated values with CARIBIC data measured near the respective trajectory position and by comparing extrapolated CARIBIC data to measurements by other experiments near the respective trajectory positions. Best agreement between extrapolated and measured data is achieved with particle lifetimes longer than the maximum length of used trajectories. The derived maps reveal regions of strong and frequent new particle formation, namely the Tropical Central and Western Africa with the adjacent Atlantic, South America, the Caribbean and Southeast Asia. These regions of particle formation coincide with those of frequent deep convective clouds. Vertical particle concentration profiles for the troposphere and the stratosphere confirm statistically previous results indicating frequent new particle formation in the tropopause region. There was no statistically significant increase in Aitken mode particle concentration between the first period of CARIBIC operation, 1997-2002, and the second period, 2004-2009. However, a significant increase in concentration occurred within the latter period when considering it in isolation.
C1 [Heintzenberg, Jost; Hermann, Markus; Weigelt, Andreas] Leibniz Inst Tropospher Res, D-04318 Leipzig, Germany.
   [Clarke, Antony; Kapustin, Vladimir] Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA.
   [Anderson, Bruce; Thornhill, Kenneth] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Van Velthoven, Peter] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
   [Zahn, Andreas] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany.
   [Brenninkmeijer, Carl] Max Planck Inst Chem, Div Atmospher Chem, D-55128 Mainz, Germany.
RP Heintzenberg, J (reprint author), Leibniz Inst Tropospher Res, Permoserstr 15, D-04318 Leipzig, Germany.
EM jost@tropos.de
RI Zahn, Andreas/K-2567-2012; Brenninkmeijer, Carl/B-6860-2013; Hermann,
   Markus/B-7527-2013
OI Zahn, Andreas/0000-0003-3153-3451; Hermann, Markus/0000-0002-5124-1571
FU German Ministry of Education and Science (AFO); European Commission
FX The authors are deeply grateful to Lufthansa Passage Airlines and
   Lufthansa Technik (in particular, Andreas Waibel, Thomas Dauer, Detlev
   Hartwig, Sven Dankert and Jorg Rohwer) for their support of CARIBIC and
   to Dieter Scharffe and Claus Koeppel (Max Planck Institute for
   Chemistry) for the equipment support and container operation. The
   development of the CARIBIC system was financially supported by the
   German Ministry of Education and Science (AFO 2000 program) and its
   operation benefited and benefits from the European Commission's DGXII
   Environment RTD 4th, 5th, 6th and 7th Framework programs.
NR 41
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PU CO-ACTION PUBLISHING
PI JARFALLA
PA RIPVAGEN 7, JARFALLA, SE-175 64, SWEDEN
SN 0280-6509
J9 TELLUS B
JI Tellus Ser. B-Chem. Phys. Meteorol.
PD NOV
PY 2011
VL 63
IS 5
BP 875
EP 890
DI 10.1111/j.1600-0889.2011.00578.x
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835IT
UT WOS:000296030800006
ER

PT J
AU Long, DA
   Okumura, M
   Miller, CE
   Hodges, JT
AF Long, D. A.
   Okumura, M.
   Miller, C. E.
   Hodges, J. T.
TI Frequency-stabilized cavity ring-down spectroscopy measurements of
   carbon dioxide isotopic ratios
SO APPLIED PHYSICS B-LASERS AND OPTICS
LA English
DT Article
ID O-2 A-BAND; HIGH-PRECISION; ABSORPTION-SPECTROSCOPY; LASER;
   SPECTROMETER; TRANSITIONS; PARAMETERS
AB Carbon dioxide (CO2) isotopic ratios on samples of pure CO2 were measured in the 1.6 mu m wavelength region using the frequency-stabilized cavity ring-down spectroscopy (FS-CRDS) technique. We present CO2 absorption spectra with peak signal-to-noise ratios as high as 28,000:1. Measured single-spectrum signal-to-noise ratios were as high as 8900:1, 10,000:1, and 1700:1 for C-13/C-12, O-18/O-16, and O-17/O-16, respectively. In addition, we demonstrate the importance of utilizing the Galatry line profile in the spectrum analysis. The use of the Voigt line profile, which neglects the observed collisional narrowing, leads to large systematic errors which are transition-dependent and vary with temperature and pressure. While the relatively low intensities of CO2 transitions near lambda=1.6 mu m make this spectral region non-optimal, the sensitivity and stability of FS-CRDS enabled measurement precision of pure CO2 samples which are comparable to those of other optical techniques which operate at far more propitious wavelengths. These results indicate that a FS-CRDS spectrometer designed to probe CO2 bands near wavelengths of 2.0 mu m or 4.3 mu m could achieve significantly improved precision over the present instrument and likely be competitive with mass spectrometric methods.
C1 [Hodges, J. T.] NIST, Chem & Biochem Reference Data Div, Gaithersburg, MD 20899 USA.
   [Long, D. A.; Okumura, M.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
   [Miller, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Hodges, JT (reprint author), NIST, Chem & Biochem Reference Data Div, 100 Bur Dr, Gaithersburg, MD 20899 USA.
EM joseph.hodges@nist.gov
RI Okumura, Mitchio/I-3326-2013
OI Okumura, Mitchio/0000-0001-6874-1137
FU National Science Foundation; National Defense Science and Engineering
   Graduate Fellowships; NASA [NNG06GD88G, NNX09AE21G]; NIST
FX David A. Long was supported by the National Science Foundation and
   National Defense Science and Engineering Graduate Fellowships. 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 (NASA). Additional support
   was provided by the Orbiting Carbon Observatory (OCO) project, a NASA
   Earth System Science Pathfinder (ESSP) mission; the NASA Upper
   Atmospheric Research Program grant NNG06GD88G and NNX09AE21G; and the
   NIST Greenhouse Gas Measurements and Climate Research Program.
NR 36
TC 17
Z9 17
U1 0
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0946-2171
EI 1432-0649
J9 APPL PHYS B-LASERS O
JI Appl. Phys. B-Lasers Opt.
PD NOV
PY 2011
VL 105
IS 2
BP 471
EP 477
DI 10.1007/s00340-011-4518-z
PG 7
WC Optics; Physics, Applied
SC Optics; Physics
GA 834DB
UT WOS:000295938100039
ER

PT J
AU Yen, JY
   Garamszegi, S
   Geisbert, JB
   Rubins, KH
   Geisbert, TW
   Honko, A
   Xia, Y
   Connor, JH
   Hensley, LE
AF Yen, Judy Y.
   Garamszegi, Sara
   Geisbert, Joan B.
   Rubins, Kathleen H.
   Geisbert, Thomas W.
   Honko, Anna
   Xia, Yu
   Connor, John H.
   Hensley, Lisa E.
TI Therapeutics of Ebola Hemorrhagic Fever: Whole-Genome Transcriptional
   Analysis of Successful Disease Mitigation
SO JOURNAL OF INFECTIOUS DISEASES
LA English
DT Article
ID NONHUMAN-PRIMATES; GENE-EXPRESSION; VIRUS INFECTION; POSTEXPOSURE
   TREATMENT; MARBURG VIRUSES; MICROARRAY DATA; IFN-ALPHA; PATHOGENESIS;
   CELLS; PROTECTION
AB The mechanisms of Ebola (EBOV) pathogenesis are only partially understood, but the dysregulation of normal host immune responses (including destruction of lymphocytes, increases in circulating cytokine levels, and development of coagulation abnormalities) is thought to play a major role. Accumulating evidence suggests that much of the observed pathology is not the direct result of virus-induced structural damage but rather is due to the release of soluble immune mediators from EBOV-infected cells. It is therefore essential to understand how the candidate therapeutic may be interrupting the disease process and/or targeting the infectious agent. To identify genetic signatures that are correlates of protection, we used a DNA microarray-based approach to compare the host genome-wide responses of EBOV-infected nonhuman primates (NHPs) responding to candidate therapeutics. We observed that, although the overall circulating immune response was similar in the presence and absence of coagulation inhibitors, surviving NHPs clustered together. Noticeable differences in coagulation-associated genes appeared to correlate with survival, which revealed a subset of distinctly differentially expressed genes, including chemokine ligand 8 (CCL8/MCP-2), that may provide possible targets for early-stage diagnostics or future therapeutics. These analyses will assist us in understanding the pathogenic mechanisms of EBOV infection and in identifying improved therapeutic strategies.
C1 [Yen, Judy Y.; Connor, John H.] Boston Univ, Sch Med, Dept Microbiol, Boston, MA 02118 USA.
   [Garamszegi, Sara; Xia, Yu; Connor, John H.] Boston Univ, Bioinformat Program, Boston, MA 02118 USA.
   [Geisbert, Joan B.; Geisbert, Thomas W.] Univ Texas Galveston, Med Branch, Dept Microbiol & Immunol, Galveston, TX 77550 USA.
   [Rubins, Kathleen H.] NASA, Houston, TX USA.
   [Honko, Anna; Hensley, Lisa E.] USA, Med Res Inst Infect Dis, Ft Detrick, MD 21702 USA.
   [Xia, Yu] Boston Univ, Dept Biomed Engn, Boston, MA 02118 USA.
   [Xia, Yu] Boston Univ, Dept Chem, Boston, MA 02118 USA.
RP Connor, JH (reprint author), Boston Univ, Sch Med, Dept Microbiol, 72 E Concord St, Boston, MA 02118 USA.
EM jhconnor@bu.edu
OI Connor, John/0000-0002-8867-7256; Xia, Yu/0000-0002-5596-5518; Honko,
   Anna/0000-0001-9165-148X
FU Joint Science and Technology Office for Chemical and Biological Defense
   [4.0021.08.RD.B]; Defense Threat Reduction Agency; Whitehead Institute
FX The Joint Science and Technology Office for Chemical and Biological
   Defense and the Defense Threat Reduction Agency, JSTO-CBD
   4.0021.08.RD.B, and the Whitehead Institute Fellows fund (to K. H. R.).
NR 37
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U1 0
U2 10
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-1899
J9 J INFECT DIS
JI J. Infect. Dis.
PD NOV 1
PY 2011
VL 204
SU 3
BP S1043
EP S1052
DI 10.1093/infdis/jir345
PG 10
WC Immunology; Infectious Diseases; Microbiology
SC Immunology; Infectious Diseases; Microbiology
GA 834VD
UT WOS:000295991400040
PM 21987740
ER

PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Untitled
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] Jet Prop Lab, Pasadena, CA 91109 USA.
   [Siegel, Peter H.] CALTECH, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA.
EM phs@caltech.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD NOV
PY 2011
VL 1
IS 2
BP 337
EP 340
DI 10.1109/TTHZ.2011.2167173
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TK
UT WOS:000208702900001
ER

PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneers A Series of Interviews With Significant Contributors
   to Terahertz Science and Technology
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
   [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
   [Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
NR 0
TC 0
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U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD NOV
PY 2011
VL 1
IS 2
BP 341
EP 341
DI 10.1109/TTHZ.2011.2168996
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TK
UT WOS:000208702900002
ER

PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneer: Paul L. Richards Working at the Edge-Transition Edge
   Sensors and the Edge of the Universe
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Biographical-Item
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91109 USA.
   [Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91109 USA.
   [Siegel, Peter H.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA.
EM phs@caltech.edu
NR 1
TC 1
Z9 1
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD NOV
PY 2011
VL 1
IS 2
BP 342
EP 348
DI 10.1109/TTHZ.2011.2168998
PG 7
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TK
UT WOS:000208702900003
ER

PT J
AU Reck, TJ
   Chen, LH
   Zhang, CH
   Arsenovic, A
   Groppi, C
   Lichtenberger, AW
   Weikle, RM
   Barker, NS
AF Reck, Theodore J.
   Chen, Lihan
   Zhang, Chunhu
   Arsenovic, Alex
   Groppi, Christopher
   Lichtenberger, Arthur W.
   Weikle, Robert M., II
   Barker, N. Scott
TI Micromachined Probes for Submillimeter-Wave On-Wafer Measurements-Part
   I: Mechanical Design and Characterization
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Coplanar waveguide; micromachining; rectangular waveguide;
   submillimeter-wave integrated circuits; submillimeter-wave measurements
AB The mechanical design and characterization of a micromachined on-wafer probe scalable to submillimeter-wave frequencies is presented. The design consists of a silicon micromachined probe with a ground-signal-ground configuration on a 15 mu m thick silicon substrate. This micromachined chip is housed in a metal waveguide block that provides mechanical support for the probe and enables coupling to a waveguide flange. Load-cell measurements of the probe show a DC contact resistance below 0.07 Omega with an applied force of 1 mN. A companion paper presents the electromagnetic design and calibrated on-wafer measurements at 500 to 750 GHz.
C1 [Reck, Theodore J.] Jet Prop Lab, Pasadena, CA 91030 USA.
   [Chen, Lihan; Zhang, Chunhu; Arsenovic, Alex; Lichtenberger, Arthur W.; Weikle, Robert M., II; Barker, N. Scott] Univ Virginia, Charles L Brown Dept Elect Engn, Charlottesville, VA 22903 USA.
   [Groppi, Christopher] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Reck, TJ (reprint author), Jet Prop Lab, Pasadena, CA 91030 USA.
EM theodore.reck@jpl.nasa.gov
RI Groppi, Christopher/L-5284-2013
OI Groppi, Christopher/0000-0002-2021-1628
FU Defense Advanced Reaserch Project Agency (DARPA) THz Electronics
   Program; Army Research Laboratory under DARPA [HR0011-09-C-0062]; Army
   Research Laboratory under Northrop Grumman; Army Research Laboratory
   under National Ground Intelligence Center [W911W5-06-C-0001]; Teledyne
   Scientific Company, LLC [G0U551521]
FX This work was supported by the Defense Advanced Reaserch Project Agency
   (DARPA) THz Electronics Program and by the Army Research Laboratory
   under DARPA Contract HR0011-09-C-0062, under a sub-contract from
   Northrop Grumman and the National Ground Intelligence Center Contract
   W911W5-06-C-0001, and by a contract from Teledyne Scientific Company,
   LLC under Contract G0U551521.
NR 28
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U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD NOV
PY 2011
VL 1
IS 2
BP 349
EP 356
DI 10.1109/TTHZ.2011.2165013
PG 8
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TK
UT WOS:000208702900004
ER

PT J
AU Reck, TJ
   Chen, LH
   Zhang, CH
   Arsenovic, A
   Groppi, C
   Lichtenberger, A
   Weikle, RM
   Barker, NS
AF Reck, Theodore J.
   Chen, Lihan
   Zhang, Chunhu
   Arsenovic, Alex
   Groppi, Christopher
   Lichtenberger, Arthur
   Weikle, Robert M., II
   Barker, N. Scott
TI Micromachined Probes for Submillimeter-Wave On-Wafer Measurements-Part
   II: RF Design and Characterization
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Coplanar waveguides; micromachining; rectangular waveguides;
   submillimeter-wave integrated circuits; submillimeter-wave measurements
AB The electromagnetic design and characterization of a micromachined submillimeter-wave on-wafer probe is presented. The mechanical design and fabrication of the probe is presented in the companion paper (Part I). Finite element simulations are applied to design an integrated probe chip to couple between rectangular waveguide and the ground-signal-ground (GSG) probe. Two designs based on different transmission line topologies are implemented and their performance assessed. The insertion loss of the probes over the WR-1.5 band measures between 6-10 dB and return loss measures from 10 to 15 dB. Offset short measurements are used to verify the performance of the probes and that they can be employed for calibrated on-wafer measurements.
C1 [Reck, Theodore J.] CALTECH, Jet Prop Lab, Pasadena, CA 91030 USA.
   [Reck, Theodore J.; Chen, Lihan; Zhang, Chunhu; Arsenovic, Alex; Lichtenberger, Arthur; Weikle, Robert M., II; Barker, N. Scott] Univ Virginia, Charles L Brown Dept Elect Engn, Charlottesville, VA 22903 USA.
   [Groppi, Christopher] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Reck, TJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91030 USA.
EM theodore.reck@jpl.nasa.gov
RI Groppi, Christopher/L-5284-2013
OI Groppi, Christopher/0000-0002-2021-1628
FU Defense Advanced Research Projects Agency (DARPA) THz Electronics
   Program; Army Research Laboratory under DARPA [HR0011-09-C-0062]; Army
   Research Laboratory under Northrop Grumman; Army Research Laboratory
   under National Ground Intelligence Center [W911W5-06-C-0001]; Teledyne
   Scientific Company, LLC [G0U551521]
FX This work was supported by the Defense Advanced Research Projects Agency
   (DARPA) THz Electronics Program and by the Army Research Laboratory
   under DARPA Contract HR0011-09-C-0062 under a sub-contract from Northrop
   Grumman and the National Ground Intelligence Center under Contract
   W911W5-06-C-0001 and a contract from Teledyne Scientific Company, LLC
   under Contract G0U551521.
NR 11
TC 30
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U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD NOV
PY 2011
VL 1
IS 2
BP 357
EP 363
DI 10.1109/TTHZ.2011.2165020
PG 7
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TK
UT WOS:000208702900005
ER

PT J
AU van Donkelaar, A
   Martin, RV
   Levy, RC
   da Silva, AM
   Krzyzanowski, M
   Chubarova, NE
   Semutnikova, E
   Cohen, AJ
AF van Donkelaar, Aaron
   Martin, Randall V.
   Levy, Robert C.
   da Silva, Arlindo M.
   Krzyzanowski, Michal
   Chubarova, Natalia E.
   Semutnikova, Eugenia
   Cohen, Aaron J.
TI Satellite-based estimates of ground-level fine particulate matter during
   extreme events: A case study of the Moscow fires in 2010
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE MODIS; PM(2.5); Moscow wildfires; Aerosol optical depth
ID AEROSOL OPTICAL-THICKNESS; UNITED-STATES; CHEMISTRY; MORTALITY;
   TRANSPORT; POLLUTION; HEALTH; DEPTH; CHINA; LAND
AB We estimate fine particulate matter (PM(2.5)) concentrations daily using MODIS satellite observations of aerosol optical depth (AOD) for a major biomass burning event around Moscow during summer 2010. Evaluation of MODIS AOD with the Moscow AERONET site supports a MODIS-AOD error estimate of +/-(0.05 + 0.2 x AOD) for this event. However, since the smoke was often thick (AOD > 4.0) and spatially variable, the standard MODIS algorithm incorrectly identifies some aerosol as cloud. We test relaxed cloud screening criteria that increase MODIS coverage by 21% and find excellent agreement with coincident operational retrievals (r(2) = 0.994, slope = 1.01) with no evidence of false aerosol detection. We relate the resultant MODIS AOD to PM(2.5) using aerosol vertical profiles from the GEOS-Chem chemical transport model. Our estimates are in good agreement with PM(2.5) values estimated from in-situ PM(10) (r(2) = 0.85, slope = 1.06), and we find that the relationship between AOD and PM2.5 is insensitive to uncertainties in biomass burning emissions. The satellite-derived and in-situ values both indicate that peak daily mean concentrations of approximately 600 mu g m(-3) occurred on August 7, 2010 in the Moscow region of the Russian Federation. We estimate that exposure to air pollution from the Moscow wildfires may have caused hundreds of excess deaths. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
   [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
   [Krzyzanowski, Michal] WHO, European Ctr Environm & Hlth, Reg Off Europe, Bonn, Germany.
   [Chubarova, Natalia E.] Moscow MV Lomonosov State Univ, Dept Geog, Moscow, Russia.
   [Semutnikova, Eugenia] Mosecomonitoring, State Environm Org, Moscow, Russia.
   [Cohen, Aaron J.] Hlth Effects Inst, Boston, MA USA.
RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, 6300 Coburg Rd, Halifax, NS B3H 3J5, Canada.
EM aaron.van.Donkelaar@dal.ca; randall.martin@dal.ca;
   robert.c.levy@nasa.gov; arlindo.m.dasilva@nasa.gov;
   mkr@ecehbonn.euro.who.int; chubarova@imp.kiae.ru; info@mosecom.ru;
   acohen@healtheffects.org
RI da Silva, Arlindo/D-6301-2012; Levy, Robert/M-7764-2013; Martin,
   Randall/C-1205-2014; Chem, GEOS/C-5595-2014
OI da Silva, Arlindo/0000-0002-3381-4030; Levy, Robert/0000-0002-8933-5303;
   Martin, Randall/0000-0003-2632-8402; 
FU Natural Science and Engineering Research Council of Canada (NSERC);
   Killam Trust
FX This work was supported by the Natural Science and Engineering Research
   Council of Canada (NSERC) and the Killam Trust.
NR 48
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U1 1
U2 32
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 NOV
PY 2011
VL 45
IS 34
BP 6225
EP 6232
DI 10.1016/j.atmosenv.2011.07.068
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 831UU
UT WOS:000295757400016
ER

PT J
AU Liu, JJ
   Zheng, YF
   Li, ZQ
   Flynn, C
   Welton, EJ
   Cribb, M
AF Liu, Jianjun
   Zheng, Youfei
   Li, Zhanqing
   Flynn, Connor
   Welton, E. J.
   Cribb, Mareen
TI Transport, vertical structure and radiative properties of dust events in
   southeast China determined from ground and space sensors
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Dust; Transport; Vertical structure; Radiative properties; Southeast
   China
ID TO-BACKSCATTER RATIO; KEY AEROSOL TYPES; ASIAN DUST; LIDAR MEASUREMENTS;
   OPTICAL-PROPERTIES; RAMAN LIDAR; ACE-ASIA; WORLDWIDE LOCATIONS;
   INDIAN-OCEAN; SURFACE
AB Two dust events were detected over the Yangtze Delta region of China during March 14-17 and April 25-26 in 2009 where such dust events are uncommon. The transport behavior, spatio-temporal evolution, vertical structure, direct radiative effects, as well as induced heating rates, are investigated using a combination of ground-based and satellite-based measurements, a back-trajectory analysis, an aerosol model and a radiative transfer model. Back-trajectories, wind fields and aerosol model analyses show that the first dust originated in northern/northwestern China and the second generated in the Taklimakan desert in northwest China, and traveled across the Hexi corridor and Loess Plateau to the Yangtze Delta region (the so-called "dust corridor"). The mean lidar extinction-to-backscatter ratio (LR) during the two dust events was 38.7 +/- 10.4 sr and 42.7 +/- 15.2 sr, respectively. The mean aerosol depolarization ratio (delta(a)) for the first dust event was 0.16 +/- 0.07, with a maximum value of 0.32. For the second, the mean delta(a) was around 0.19 +/- 0.06, with a maximum value of 0.29. Aerosol extinction coefficient and da profiles for the two events were similar: two aerosol layers consisting of dust aerosols and a mixture of dust and anthropogenic pollution aerosols. The topmost aerosol layer is above 3.5 km. The maximum mean aerosol extinction coefficients were 0.5 km(-1) and 0.54 km(-1) at about 0.7 km and 1.1 km, respectively. Significant effects of cooling at the surface and heating in the atmosphere were found during these dust events. Diurnal mean shortwave radiative forcings (efficiencies) at the surface, the top-of-the-atmosphere and within the atmosphere were -36.8 (-80.0), -13.6 (-29.6) and 23.2 (50.4) W m(-2), respectively, during the first dust event, and -48.2 (-70.9), -21.4 (-31.5) and 26.8 (39.4) W m(-2), respectively, during the second dust event. Maximum heating rates occurred at 0.7 km during the first dust event and at 1.1 km during the second dust event, with a maximum value of 2.74 K day(-1) for each case. This significant atmospheric heating induced by elevated dust aerosol layers can affect convection and stability in the lower troposphere. Published by Elsevier Ltd.
C1 [Liu, Jianjun; Zheng, Youfei; Li, Zhanqing] Nanjing Univ Informat Sci & Technol, Jiangsu Key Lab Atmospher Environm Monitoring & P, Nanjing, Peoples R China.
   [Liu, Jianjun; Li, Zhanqing; Cribb, Mareen] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
   [Liu, Jianjun; Li, Zhanqing; Cribb, Mareen] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
   [Flynn, Connor] Pacific NW Natl Lab, Richland, WA 99352 USA.
   [Welton, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Li, ZQ (reprint author), Beijing Normal Univ, Lab Earth Surface Proc & Resource Ecol, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
EM zli@atmos.umd.edu
RI Welton, Ellsworth/A-8362-2012; Liu, Jianjun/F-4673-2014; Li,
   Zhanqing/F-4424-2010; Cribb, Maureen/K-1341-2013
OI Li, Zhanqing/0000-0001-6737-382X; Cribb, Maureen/0000-0002-9745-3676
FU National Basic Research Program of China [2006CB403705, 2011CB403405];
   DOE [DEFG0208ER64571]; NASA [NNX08AH71G]
FX This study was supported by the National Basic Research Program of China
   (2006CB403705 and 2011CB403405), DOE (DEFG0208ER64571), and NASA
   (NNX08AH71G).
NR 57
TC 18
Z9 20
U1 1
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 NOV
PY 2011
VL 45
IS 35
BP 6469
EP 6480
DI 10.1016/j.atmosenv.2011.04.031
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 830JR
UT WOS:000295653800022
ER

PT J
AU Morel, AC
   Saatchi, SS
   Malhi, Y
   Berry, NJ
   Banin, L
   Burslem, D
   Nilus, R
   Ong, RC
AF Morel, Alexandra C.
   Saatchi, Sassan S.
   Malhi, Yadvinder
   Berry, Nicholas J.
   Banin, Lindsay
   Burslem, David
   Nilus, Reuben
   Ong, Robert C.
TI Estimating aboveground biomass in forest and oil palm plantation in
   Sabah, Malaysian Borneo using ALOS PALSAR data
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE ALOS-PALSAR; Land-cover monitoring; Aboveground biomass; Oil palm;
   Borneo
ID BRAZILIAN AMAZONIA; TROPICAL FORESTS; POLARIMETRIC SAR; CARBON STOCKS;
   WOOD DENSITY; TREE BIOMASS; LAND-USE; RADAR; CLASSIFICATION; JERS-1
AB Conversion of tropical forests to oil palm plantations in Malaysia and Indonesia has resulted in large-scale environmental degradation, loss of biodiversity and significant carbon emissions. For both countries to participate in the United Nation's REDD (Reduced Emission from Deforestation and Degradation) mechanism, assessment of forest carbon stocks, including the estimated loss in carbon from conversion to plantation, is needed. In this study, we use a combination of field and remote sensing data to quantify both the magnitude and the geographical distribution of carbon stock in forests and timber plantations, in Sabah, Malaysia, which has been the site of significant expansion of oil palm cultivation over the last two decades. Forest structure data from 129 ha of research and inventory plots were used at different spatial scales to discriminate forest biomass across degradation levels. Field data was integrated with ALOS PALSAR (Advanced Land-Observing Satellite Phased Array L-band Synthetic Aperture Radar) imagery to both discriminate oil palm plantation from forest stands, with an accuracy of 97.0% (kappa = 0.64) and predict AGB using regression analysis of HV-polarized PALSAR data (R-2 = 0.63, p <.001). Direct estimation of AGB from simple regression models was sensitive to both environmental conditions and forest structure. Precipitation effect on the backscatter data changed the HV prediction of AGB significantly (R-2 = 0.21, p <.001), and scattering from large leaves of mature palm trees significantly impeded the use of a single HV-based model for predicting AGB in palm oil plantations. Multi-temporal SAR data and algorithms based on forest types are suggested to improve the ability of a sensor similar to ALOS PALSAR for accurately mapping and monitoring forest biomass, now that the ALOS PALSAR sensor is no longer operational. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Morel, Alexandra C.; Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England.
   [Saatchi, Sassan S.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Berry, Nicholas J.] Ecometrica, Edinburgh EH9 1PJ, Midlothian, Scotland.
   [Banin, Lindsay] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
   [Burslem, David] Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland.
   [Nilus, Reuben; Ong, Robert C.] Forest Res Ctr, Sabah Forestry Dept, Sandakan, Sabah, Malaysia.
RP Morel, AC (reprint author), Columbia Univ, Earth Inst, Low Lib 405, MC 4335,535 W 116th St, New York, NY 10027 USA.
EM alexandra.morel@gmail.com
RI Malhi, Yadvinder/I-4668-2012; 
OI Burslem, David/0000-0001-6033-0990
NR 65
TC 65
Z9 68
U1 5
U2 79
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD NOV 1
PY 2011
VL 262
IS 9
BP 1786
EP 1798
DI 10.1016/j.foreco.2011.07.008
PG 13
WC Forestry
SC Forestry
GA 831TV
UT WOS:000295754900015
ER

PT J
AU Passchier, S
   Browne, G
   Field, B
   Fielding, CR
   Krissek, LA
   Panter, K
   Pekar, SF
   Harwood
   Florindo, F
   Levy, R
   Acton, G
   Atkins, C
   Bassett, K
   Berg, M
   Bibby, T
   Blair, S
   Blank, L
   Del Carlo, P
   Dooley, J
   Drew, S
   Dunbar, G
   Frank, T
   Frisch-Gleason, R
   Grelle, T
   Handwerger, D
   Hannah, M
   Hoffmann, S
   Hubbard, J
   Huffman, L
   Ishman, S
   Johnson, K
   Jovane, L
   Konfirst, M
   Kuhn, G
   Lacy, L
   Lehmann, R
   Magens, D
   Mankoff, K
   Millan, C
   Nielsen, S
   Olney, M
   Patterson, T
   Paulsen, T
   Persico, D
   Petrushak, S
   Pierdominici, S
   Pound, K
   Reed, J
   Reichelt, L
   Riesselman, C
   Sandroni, S
   Schmitt, D
   di Clemente, GS
   Speece, M
   Strada, E
   Szymcek, P
   Talarico, F
   Taviani, M
   Tuzzi, E
   Williams, R
   Wonik, T
AF Passchier, S.
   Browne, G.
   Field, B.
   Fielding, C. R.
   Krissek, L. A.
   Panter, K.
   Pekar, S. F.
   Harwood, David
   Florindo, Fabio
   Levy, Richard (Rich)
   Acton, Gary
   Atkins, Clifford (Cliff)
   Bassett, Kari
   Berg, Megan
   Bibby, Theodore (Ted)
   Blair, Stacie
   Blank, Leslie
   Del Carlo, Paola
   Dooley, Julia
   Drew, Scott
   Dunbar, Gavin
   Frank, Tracy
   Frisch-Gleason, Robin
   Grelle, Thomas
   Handwerger, David (Dave)
   Hannah, Michael (Mike)
   Hoffmann, Stefan
   Hubbard, Joanna
   Huffman, Louise
   Ishman, Scott
   Johnson, Katherine (Katie)
   Jovane, Luigi
   Konfirst, Matthew (Matt)
   Kuhn, Gerhard (Gerd)
   Lacy, Laura
   Lehmann, Rainer
   Magens, Diana
   Mankoff, Kenneth (Ken)
   Millan, Cristina
   Nielsen, Simon
   Olney, Matthew (Matt)
   Patterson, Taylor
   Paulsen, Timothy (Tim)
   Persico, Davide
   Petrushak, Steven (Steve)
   Pierdominici, Simona
   Pound, Katherine (Kate)
   Reed, Joshua (Josh)
   Lucia (Lucy)
   Riesselman, Christina
   Sandroni, Sonia
   Schmitt, Douglas (Doug)
   di Clemente, Graziano Scotto
   Speece, Marvin (Marv)
   Strada, Eleonora
   Szymcek, Phillip (Phill)
   Talarico, Franco
   Taviani, Marco
   Tuzzi, Eva
   Williams, Robert (Bob)
   Wonik, Thomas
CA ANDRILL-SMS Sci Team
TI Early and middle Miocene Antarctic glacial history from the sedimentary
   facies distribution in the AND-2A drill hole, Ross Sea, Antarctica
SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN
LA English
DT Article
ID ATMOSPHERIC CARBON-DIOXIDE; ICE-SHEET; MCMURDO SOUND; GLACIMARINE
   SEDIMENTATION; TRANSANTARCTIC MOUNTAINS; EAST ANTARCTICA; RETREAT
   HISTORY; GROUNDING LINE; SHELF; MAXIMUM
AB In 2007, the Antarctic Geological Drilling Program (ANDRILL) drilled 1138.54 m of strata similar to 10 km off the East Antarctic coast, including an expanded early to middle Miocene succession not previously recovered from the Antarctic continental shelf. Here, we present a facies model, distribution, and paleoclimatic interpretation for the AND-2A drill hole, which enable us, for the first time, to reconstruct periods of early and middle Miocene glacial advance and retreat and paleo environmental changes at an ice-proximal site. Three types of facies associations can be recognized that imply significantly different paleoclimatic interpretations. (1) A diamictite-dominated facies association represents glacially dominated depositional environments, including subglacial environments, with only brief intervals where ice-free coasts existed, and periods when the ice sheet was periodically larger than the modern ice sheet. (2) A stratified diamictite and mudstone facies association includes facies characteristic ofopen-marine to iceberg-influenced depositional environments and is more consistent with a very dynamic ice sheet, with a grounding line south of the modern position. (3) A mudstone-dominated facies association generally lacks diamictites and was produced in a glacially influenced hemipelagic depositional environment. Based on the distribution of these facies associations, we can conclude that the Antarctic ice sheets were dynamic, with grounding lines south of the modern location at ca. 20.1-19.6 Ma and ca. 19.3-18.7 Ma and during the Miocene climatic optimum, ca. 17.6-15.4 Ma, with ice-sheet and sea-ice minima at ca. 16.5-16.3 Ma and ca. 15.7-15.6 Ma. While glacial minima at ca. 20.1-19.6 Ma and ca. 19.3-18.7 Ma were characterized by temperate margins, an increased abundance of gravelly facies and diatomaceous siltstone and a lack of meltwater plume deposits suggest a cooler and drier climate with polythermal conditions for the Miocene climatic optimum (ca. 17.6-15.4 Ma). Several periods of major ice growth with a grounding line traversing the drill site are recognized between ca. 20.2 and 17.6 Ma, and after ca. 15.4 Ma, with evidence of cold polar glaciers with ice shelves. The AND-2A core provides proximal evidence that during the middle Miocene climate transition, an ice sheet larger than the modern ice sheet was already present by ca. 14.7 Ma, similar to 1 m.y. earlier than generally inferred from deep-sea oxygen isotope records. These findings highlight the importance of high-latitude ice-proximal records for the interpretation of far-field proxies across major climate transitions.
C1 [Passchier, S.] Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA.
   [Passchier, S.] Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA.
   [Browne, G.; Field, B.] GNS Sci, Lower Hutt 5040, New Zealand.
   [Fielding, C. R.] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.
   [Krissek, L. A.; Drew, Scott; Millan, Cristina] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
   [Panter, K.] Bowling Green State Univ, Dept Geol, Bowling Green, OH 43403 USA.
   [Pekar, S. F.] CUNY Queens Coll, Sch Earth & Environm Sci, Flushing, NY 11367 USA.
   [Harwood, David; Huffman, Louise; Lacy, Laura; Reed, Joshua (Josh)] Univ Nebraska, ANDRILL Sci Management Off, Lincoln, NE 68588 USA.
   [Florindo, Fabio] Ist Nazl Geofis, I-00143 Rome, Italy.
   [Acton, Gary] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
   [Atkins, Clifford (Cliff)] Victoria Univ Wellington, Sch Geog Environm & Earth Sci, Wellington 6005, New Zealand.
   [Bassett, Kari] Univ Canterbury, Dept Geol Sci, Christchurch, New Zealand.
   [Bibby, Theodore (Ted); Blair, Stacie; Petrushak, Steven (Steve)] Florida State Univ, Dept Geol Sci, Tallahassee, FL 32306 USA.
   [Blank, Leslie] Raytheon Polar Serv, Centennial, CO USA.
   [Del Carlo, Paola] Ist Nazl Geofis & Vulcanol, Sezione Pisa, I-56126 Pisa, Italy.
   [Dunbar, Gavin] Victoria Univ Wellington, Antarctic Res Ctr, Wellington 6005, New Zealand.
   [Frank, Tracy; Tuzzi, Eva] Univ Nebraska Lincoln, Dept Geosci, Lincoln, NE 68588 USA.
   [Grelle, Thomas; Wonik, Thomas] LIAG, Hannover, Germany.
   [Hannah, Michael (Mike)] Victoria Univ Wellington, Sch Earth Sci, Wellington 4007, New Zealand.
   [Hoffmann, Stefan] Univ Gottingen, Dept Sedimentol & Environm Geol, D-37077 Gottingen, Germany.
   [Ishman, Scott] SO Illinois Univ Carbondale, Dept Geol, Carbondale, IL 62901 USA.
   [Johnson, Katherine (Katie)] Geomarine Res, Auckland 1072, New Zealand.
   [Jovane, Luigi] Univ Calif Davis, Paleomagnet Lab, Dept Geol, Davis, CA 95616 USA.
   [Konfirst, Matthew (Matt)] No Illinois Univ, Dept Geol & Environm Geosci, De Kalb, IL 60115 USA.
   [Magens, Diana] Alfred Wegener Inst, Dept Marine Geophys, D-27515 Bremerhaven, Germany.
   [Mankoff, Kenneth (Ken)] NASA GISS, New York, NY 10025 USA.
   [Nielsen, Simon] Japan Agcy Marine Earth Sci & Technol, Ctr Deep Earth Explorat, Yokohama, Kanagawa 2360001, Japan.
   [Olney, Matthew (Matt)] Univ S Florida, Dept Geol, Tampa, FL 33620 USA.
   [Patterson, Taylor; Speece, Marvin (Marv)] Montana Tech Univ Montana, Dept Geophys Engn, Butte, MT 59701 USA.
   [Paulsen, Timothy (Tim)] Univ Wisconsin Oshkosh, Dept Geol, Oshkosh, WI 54901 USA.
   [Persico, Davide] Univ Parma, Dipartimento Sci Terra, I-43100 Parma, Italy.
   [Pierdominici, Simona] Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy.
   [Pound, Katherine (Kate)] St Cloud State Univ, Dept Earth & Atmospher Sci, St Cloud, MN 56301 USA.
   [Lucia (Lucy)] Alfred Wegener Inst, D-27568 Bremerhaven, Germany.
   [Riesselman, Christina] Stanford Univ, Geol & Environm Sci, Stanford, CA 94305 USA.
   [Sandroni, Sonia] Sez Sci Terra Siena, Museo Nazl Antartide, I-53100 Siena, Italy.
   [Schmitt, Douglas (Doug)] Univ Alberta, Inst Geophys Res, Dept Phys, Edmonton, AB T6G 2G7, Canada.
   [di Clemente, Graziano Scotto] Secondary school Luigi Stefanini, I-31100 Treviso, Italy.
   [Strada, Eleonora; Talarico, Franco] Univ Siena, Dipartimento Sci Terra, I-53100 Siena, Italy.
   [Taviani, Marco] CNR, ISMAR Bologna, I-40129 Bologna, Italy.
RP Passchier, S (reprint author), Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA.
EM passchiers@mail.montclair.edu; G.Browne@gns.cri.nz;
   brad.field@gns.cri.nz; cfielding2@unl.edu; krissek@mps.ohio-state.edu;
   kpanter@bgsu.edu; stephen.pekar@qc.cuny.edu; dharwood1@unl.edu;
   florindo@ingv.it; gdacton@ucdavis.edu; cliff.atkins@vuw.ac.nz;
   kari.bassett@canterbury.ac.nz; meganberg@mac.com; tcb03c@fsu.edu;
   blair@quartz.gly.fsu.edu; delcarlo@pi.ingv.it;
   dooleyj@christina.k12.de.us; drew.37@osu.edu; gavin.dunbar@vuw.ac.nz;
   tfrank2@unl.edu; gleason@aaps.k12.mi.us; t.grelle@liag-hannover.de;
   dave@xmission.com; Michael.hannah@vuw.ac.nz;
   s.hoffmann@geo.uni-goettingen.de; hubbard_joanna@asdk12.org;
   lhuffman@andrill.org; sishman@siu.edu; k.johnson@geomarine.org.nz;
   jovane@geology.ucdavis.edu; mk@mattkonfirst.com; llacy2@unl.edu;
   rainer.lehmann@gmx.net; Diana.Magens@awi.de; mankoff@giss.nasa.gov;
   millan.2@osu.edu; simon.n@jamstec.go.jp; cyclingolney@yahoo.co.uk;
   paulsen@uwosh.edu; davide.persico@unipr.it; gneissguy2000@yahoo.com;
   pierdominici@ingv.it; kspound@stcloudstate.edu; jareed@andrill.org;
   lreichelt@gmx.de; criessel@stanford.edu; sandroni@unisi.it;
   doug@phys.ualberta.ca; grscott@tin.it; mspeece@mtech.edu;
   strada2@unisi.it; pszymcek@gmail.com; talarico@unisi.it;
   marco.taviani@bo.ismar.cnr.it; evatuzzi@libero.it; bbermk@xtra.co.nz;
   Thomas.wonik@liag-hannover.de
RI Passchier, Sandra/B-1993-2008; Field, Brad/F-1062-2011; Panter,
   Kurt/B-4486-2010; Jovane, Luigi/E-7536-2012; Acton, Gary/B-6108-2016
OI Passchier, Sandra/0000-0001-7204-7025; Jovane,
   Luigi/0000-0003-4348-4714; 
FU National Science Foundation [0342484]; U.S. Antarctic Program (USAP);
   Raytheon Polar Services Corporation (RPSC); Antarctica New Zealand; U.S.
   National Science Foundation; New Zealand Foundation for Research;
   Italian Antarctic Research Program; German Science Foundation; Alfred
   Wegener Institute
FX This material is based upon work supported by the National Science
   Foundation under Cooperative Agreement 0342484 through subawards
   administered by the Antarctic Geologic Drilling (ANDRILL) Science
   Management Office at the University of Nebraska-Lincoln as part of the
   ANDRILL U. S. Science Support Program. Any opinions, findings, and
   conclusions or recommendations expressed in this material are those of
   the authors and do not necessarily reflect the views of the National
   Science Foundation.r The ANDRILL Program is a multinational
   collaboration among the Antarctic programs of Germany, Italy, New
   Zealand, and the United States. Antarctica New Zealand is the project
   operator and developed the drilling system in collaboration with Alex
   Pyne at Victoria University of Wellington and Webster Drilling and
   Exploration. The U.S. Antarctic Program (USAP) and Raytheon Polar
   Services Corporation (RPSC) supported the science team at McMurdo
   Station and in the Crary Science and Engineering Laboratory, while
   Antarctica New Zealand supported the drilling team at Scott Base.
   Scientific studies for the ANDRILL Program are jointly supported by the
   U.S. National Science Foundation, New Zealand Foundation for Research,
   the Italian Antarctic Research Program, the German Science Foundation,
   and the Alfred Wegener Institute.
NR 79
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U1 3
U2 23
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0016-7606
EI 1943-2674
J9 GEOL SOC AM BULL
JI Geol. Soc. Am. Bull.
PD NOV-DEC
PY 2011
VL 123
IS 11-12
BP 2352
EP 2365
DI 10.1130/B30334.1
PG 14
WC Geosciences, Multidisciplinary
SC Geology
GA 827CC
UT WOS:000295402600015
ER

PT J
AU Long, DA
   Havey, DK
   Yu, SS
   Okumura, M
   Miller, CE
   Hodges, JT
AF Long, D. A.
   Havey, D. K.
   Yu, S. S.
   Okumura, M.
   Miller, C. E.
   Hodges, J. T.
TI O-2 A-band line parameters to support atmospheric remote sensing. Part
   II: The rare isotopologues
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Oxygen; A-band; Cavity ring-down spectroscopy; Remote sensing;
   Isotopologue; Isotope; Galatry profile
ID RING-DOWN SPECTROSCOPY; SUBMILLIMETER-WAVE SPECTRUM;
   MICROWAVE-ABSORPTION LINES; MOLECULAR-OXYGEN; TRANSITION-PROBABILITY;
   HIGH-PRECISION; INTENSITIES; O-18(2); (OO)-O-16-O-18; DATABASE
AB Frequency-stabilized cavity ring-down spectroscopy (FS-CRDS) was employed to measure over 100 transitions in the R-branch of the b(1)Sigma(+)(g) <- X-3 Sigma(-)(g)(0,0) band for the rare O-2 isotopologues. The use of O-17- and O-18-enriched mixtures allowed for line positions to be measured for the (OO)-O-16-O-17, (OO)-O-16-O-18, O-17(2), (OO)-O-17-O-18, and O-18(2) isotopologues. Simultaneous fits to the upper and lower states were performed for each isotopologue using the FS-CRDS positions supplemented by microwave, millimeter, submillimeter, terahertz, and Raman ground state positions from the literature. Positions, line intensities, pressure broadening parameters, and collisional narrowing parameters are reported for the (OO)-O-16-O-18 and (OO)-O-16-O-17 isotopologues which are based upon the present study and our earlier FS-CRDS work (Long et al. J Quant Spectrosc Radiat Transfer 2010;111:2021 [18] and Robichaud et al. J Phys Chem A 2009;113:13089 [15]). The calculated line intensities include a term for the observed Herman-Wallis-like interaction and correct a frequency-dependent error, which is present in current spectroscopic databases. Published by Elsevier Ltd.
C1 [Hodges, J. T.] Natl Inst Stand & Technol, Chem & Biochem Reference Data Div, Gaithersburg, MD 20899 USA.
   [Long, D. A.; Okumura, M.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
   [Havey, D. K.] James Madison Univ, Dept Chem & Biochem, Harrisonburg, VA 22807 USA.
   [Yu, S. S.; Miller, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hodges, JT (reprint author), Natl Inst Stand & Technol, Chem & Biochem Reference Data Div, 100 Bur Dr, Gaithersburg, MD 20899 USA.
EM joseph.hodges@nist.gov
RI Okumura, Mitchio/I-3326-2013; Yu, Shanshan/D-8733-2016
OI Okumura, Mitchio/0000-0001-6874-1137; 
FU National Defense Science and Engineering Graduate Fellowship; National
   Science Foundation; National Research Council; National Aeronautics and
   Space Administration (NASA); Orbiting Carbon Observatory (OCO), a NASA
   Earth System Science Pathfinder (ESSP) mission; NASA [NNG06GD88G,
   NNX09AE21G]; NIST
FX David A. Long was supported by the National Defense Science and
   Engineering Graduate Fellowship and the National Science Foundation
   Graduate Fellowship. Daniel K. Havey acknowledges the support of the
   National Research Council as a postdoctoral fellow at the National
   Institute of Science and Technology (NIST), Gaithersburg, MD. 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 (NASA). Additional support
   was provided by the Orbiting Carbon Observatory (OCO) project, a NASA
   Earth System Science Pathfinder (ESSP) mission; the NASA Upper
   Atmospheric Research Program Grant NNG06GD88G and NNX09AE21G; and the
   NIST Greenhouse Gas Measurements and Climate Research Program. We would
   also like to acknowledge Dr. Mona Shahgholi for performing the described
   mass spectral analysis.
NR 53
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U1 0
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD NOV
PY 2011
VL 112
IS 16
BP 2527
EP 2541
DI 10.1016/j.jqsrt.2011.07.002
PG 15
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 831XF
UT WOS:000295763700001
ER

PT J
AU Spurr, R
   Natraj, V
AF Spurr, R.
   Natraj, V.
TI A linearized two-stream radiative transfer code for fast approximation
   of multiple-scatter fields
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE 2-Stream; Radiative transfer; Jacobians; Multiple-scatter accuracy
ID TRANSFER MODEL; ADJOINT PERTURBATION; WEIGHTING FUNCTIONS; LAYERED
   MEDIA; ALGORITHM; RETRIEVAL; ACCURACY; GOME; BAND
AB Performance is an issue for radiative transfer simulations in hyper-spectral remote sensing backscatter retrieval algorithms. 2-Stream models are often used to speed up flux and radiance calculations. Here we present a linearized 2-stream multiple-scatter code, with the ability to generate analytic weighting functions with respect to any atmospheric or surface property. We examine 2-stream accuracy for the satellite intensity diffuse field, and the corresponding Jacobians for total ozone column and surface albedo, for an application in the ozone UV Huggins bands. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Spurr, R.] RT Solut Inc, Cambridge, MA 02138 USA.
   [Natraj, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Spurr, R (reprint author), RT Solut Inc, 9 Channing St, Cambridge, MA 02138 USA.
EM rtsolutions@verizon.net
FU National Aeronautics and Space Administration
FX This work was performed for the Orbiting Carbon Observatory Project at
   the Jet Propulsion Laboratory, California Institute of Technology, under
   a contract with the National Aeronautics and Space Administration.
NR 24
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U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD NOV
PY 2011
VL 112
IS 16
BP 2630
EP 2637
DI 10.1016/j.jqsrt.2011.06.014
PG 8
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 831XF
UT WOS:000295763700010
ER

PT J
AU Baker, JD
   Becker, BL
   Wurth, TA
   Johanos, TC
   Littnan, CL
   Henderson, JR
AF Baker, J. D.
   Becker, B. L.
   Wurth, T. A.
   Johanos, T. C.
   Littnan, C. L.
   Henderson, J. R.
TI Translocation as a tool for conservation of the Hawaiian monk seal
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE Translocation; Relocation; Hawaiian monk seal; Survival; Dispersal
ID MONACHUS-SCHAUINSLANDI; POPULATIONS; SUCCESS; REHABILITATION; ANIMALS;
   ISLAND
AB The deteriorating demographic status of the endangered Hawaiian monk seal has motivated renewed and expanded proposals for conservation action, including translocation of seals to improve survival. Over the past three decades, numerous monk seal translocations have been conducted with a variety of objectives, including mitigating shark predation and conspecific male aggression, reducing human-seal interactions, and taking advantage of favorable foraging habitats to improve survival. Here, we analyze our cumulative experience with translocation of Hawaiian monk seals. We found a strong correlation between the time seals remained in the vicinity of the release site and their age. Recently weaned pups (with little or no at-sea foraging experience) exhibited high fidelity to release sites commensurate with that shown by untranslocated pups to their birth location. In contrast, juvenile and adult seals tended to stray from their release locations farther and sooner. Nevertheless, when 21 adult male seals were moved more than 1000 km from Laysan Island in the Northwestern Hawaiian Islands (NWHI), to the main Hawaiian Islands (MHI), they subsequently dispersed among the MHI; however, only one was observed to return to the NWHI. Translocated seals appeared to survive at rates comparable to seals native to the release site. Outcomes suggest that in most cases the intended objectives of translocations were achieved. Except for one notable case, translocations within the MHI to arrest human-seal interactions were mostly unsuccessful. These findings will be essential for informing successful large-scale translocation plans in the future. Published by Elsevier Ltd.
C1 [Baker, J. D.; Becker, B. L.; Johanos, T. C.; Littnan, C. L.; Henderson, J. R.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96814 USA.
   [Wurth, T. A.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
RP Baker, JD (reprint author), NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1601 Kapiolani Blvd,Suite 1110, Honolulu, HI 96814 USA.
EM jason.baker@noaa.gov; brenda.becker@noaa.gov; tracy.wurth@noaa.gov;
   thea.johanos-kam@noaa.gov; charles.littnan@noaa.gov;
   john.r.henderson@noaa.gov
NR 48
TC 11
Z9 11
U1 8
U2 87
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
J9 BIOL CONSERV
JI Biol. Conserv.
PD NOV
PY 2011
VL 144
IS 11
BP 2692
EP 2701
DI 10.1016/j.biocon.2011.07.030
PG 10
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 827QL
UT WOS:000295442900018
ER

PT J
AU Gloor, M
   Bellan, J
AF Gloor, Michael
   Bellan, Josette
TI A new formulation of the Large Eddy Simulation composition equations for
   two-phase fully-multicomponent turbulent flows
SO COMPUTERS & FLUIDS
LA English
DT Article
DE Large Eddy Simulation; Two-phase flows; Multicomponent; Mixing layer;
   Fully-multicomponent flows
ID DIRECT NUMERICAL-SIMULATION; APPROXIMATE DECONVOLUTION MODEL;
   SUBGRID-SCALE MODELS; PLANE MIXING LAYER; EVAPORATING DROPS; LADEN;
   THERMODYNAMICS; MIXTURES; STREAM; PHASE
AB The Large Eddy Simulation (LES) composition equations for fully multicomponent two-phase flows are here reformulated compared to a previous study in order to palliate modeling issues identified with the previous formulation. These modeling issues were highlighted in an a priori study using a Direct Numerical Simulation (DNS) database of a transitional, compressible, gaseous, temporal mixing layer laden with evaporating fuel drops. The issues consisted of: (1) the dominance of resolved source terms (representing the effect of the drops on the gas) with respect to advection and (2) the important role of subgrid source terms, even when the filter width was moderate with respect to the DNS grid spacing (e.g. factor of 4). The new formulation no longer exhibits the first issue, while the second issue is only present at larger filter widths (e.g. larger than a factor of 8). The capability to model SGS effects other than those resulting from source terms is a priori tested on this new formulation for two different SGS models using the DNS database. Due to more accurate modeling possibilities and improved computational efficiency, the new set of equations is identified as better suited for LES applications. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Bellan, Josette] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Gloor, Michael] Swiss Fed Inst Technol, Inst Fluid Dynam, CH-8092 Zurich, Switzerland.
RP Bellan, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM josette.bellan@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX This study was conducted at the Jet Propulsion Laboratory (JPL) of the
   California Institute of Technology (Caltech) under partial sponsorship
   of the National Aeronautics and Space Administration (NASA) Fundamental
   Aeronautics program. The computational resources were provided by the
   JPL and NASA AMES Supercomputing Centers.
NR 27
TC 0
Z9 0
U1 2
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-7930
J9 COMPUT FLUIDS
JI Comput. Fluids
PD NOV
PY 2011
VL 50
IS 1
BP 94
EP 103
DI 10.1016/j.compfluid.2011.06.017
PG 10
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 826HH
UT WOS:000295344700009
ER

PT J
AU Inan, OT
   Marcu, O
   Sanchez, ME
   Bhattacharya, S
   Kovacs, GTA
AF Inan, Omer T.
   Marcu, Oana
   Sanchez, Max E.
   Bhattacharya, Sharmila
   Kovacs, Gregory T. A.
TI A portable system for monitoring the behavioral activity of Drosophila
SO JOURNAL OF NEUROSCIENCE METHODS
LA English
DT Article
DE Locomotor behavior; Shaking behavior; Drosophila melanogaster; Activity
   monitor
ID TEMPERATURE CYCLES; LOCOMOTOR-ACTIVITY; MELANOGASTER; CAFFEINE; LIGHT;
   SYNCHRONIZATION; MUTATION; RECEPTOR; NEURONS; CLOCK
AB We describe a low-cost system for monitoring the behavioral activity of the fruit fly, Drosophila melanogaster. The system is readily adaptable to one or more cameras for simultaneous recordings of behavior from different angles and can be used for monitoring multiple individuals in a population at the same time. Signal processing allows discriminating between active and inactive periods during locomotion or flying, and quantification of subtler movements related to changes in position of the wings or legs. The recordings can be taken continuously over long periods of time and can thus provide information about the dynamics of a population. The system was used to monitor responses to caffeine, changes in temperature and g-force, and activity in a variable size population. Published by Elsevier B.V.
C1 [Inan, Omer T.; Kovacs, Gregory T. A.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
   [Marcu, Oana] SETI Inst, Mountain View, CA 94043 USA.
   [Marcu, Oana; Sanchez, Max E.; Bhattacharya, Sharmila] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
RP Bhattacharya, S (reprint author), NASA, Ames Res Ctr, Mail Stop 236-5, Moffett Field, CA 94035 USA.
EM sharmila.bhattacharya@nasa.gov
FU National Aeronautics and Space Administration's (NASA) National Center
   for space Biological Technologies [NNA04CC32A]; NASA [FSB-NNH09ZTT003N];
   Stanford University
FX This work was supported by the National Aeronautics and Space
   Administration's (NASA) National Center for space Biological
   Technologies under Cooperative Agreement NNA04CC32A and by NASA grant
   FSB-NNH09ZTT003N to SB. For the later phases of the work, O.T. Inan was
   supported by the G.J. Lieberman Fellowship at Stanford University. The
   authors thank John Hines (NASA) and the Lieberman family (Stanford) for
   their generous support, as well as Bob Ricks (NASA), Mozziyar Etemadi
   (UCSF), Mario Goins, and Laurent Giovangrandi (Stanford) for their
   valuable technical advice and Chris Countryman (Countryman Associates)
   for help with mechanical prototyping.
NR 28
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U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-0270
J9 J NEUROSCI METH
JI J. Neurosci. Methods
PD OCT 30
PY 2011
VL 202
IS 1
BP 45
EP 52
DI 10.1016/j.jneumeth.2011.08.039
PG 8
WC Biochemical Research Methods; Neurosciences
SC Biochemistry & Molecular Biology; Neurosciences & Neurology
GA 840CC
UT WOS:000296414900006
PM 21907735
ER

PT J
AU Matsui, H
   Kondo, Y
   Moteki, N
   Takegawa, N
   Sahu, LK
   Koike, M
   Zhao, Y
   Fuelberg, HE
   Sessions, WR
   Diskin, G
   Anderson, BE
   Blake, DR
   Wisthaler, A
   Cubison, MJ
   Jimenez, JL
AF Matsui, H.
   Kondo, Y.
   Moteki, N.
   Takegawa, N.
   Sahu, L. K.
   Koike, M.
   Zhao, Y.
   Fuelberg, H. E.
   Sessions, W. R.
   Diskin, G.
   Anderson, B. E.
   Blake, D. R.
   Wisthaler, A.
   Cubison, M. J.
   Jimenez, J. L.
TI Accumulation-mode aerosol number concentrations in the Arctic during the
   ARCTAS aircraft campaign: Long-range transport of polluted and clean air
   from the Asian continent
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LASER-INDUCED INCANDESCENCE; CLOUD CONDENSATION NUCLEI; BOUNDARY-LAYER
   CLOUDS; AIRBORNE OBSERVATIONS; INTEX-B; GLOBAL PRECIPITATION;
   TROPOSPHERIC AEROSOL; SIZE DISTRIBUTIONS; LIDAR MEASUREMENTS; POLAR
   SUNRISE
AB We evaluate the impact of transport from midlatitudes on aerosol number concentrations in the accumulation mode (light-scattering particles (LSP) with diameters > 180 nm) in the Arctic during the Arctic Research of the Composition of the Troposphere from Aircraft and Satellites (ARCTAS) campaign. We focus on transport from the Asian continent. We find marked contrasts in the number concentration (N-LSP), transport efficiency (TEN_LSP, the fraction transported from sources to the Arctic), size distribution, and the chemical composition of aerosols between air parcels from anthropogenic sources in East Asia (Asian AN) and biomass burning sources in Russia and Kazakhstan (Russian BB). Asian AN air had lower N-LSP and TEN_LSP (25 cm(-3) and 18% in spring and 6.2 cm(-3) and 3.0% in summer) than Russian BB air (280 cm(-3) and 97% in spring and 36 cm(-3) and 7.6% in summer) due to more efficient wet scavenging during transport from East Asia. Russian BB in this spring is the most important source of accumulation-mode aerosols over the Arctic, and BB emissions are found to be the primary source of aerosols within all the data in spring during ARCTAS. On the other hand, the contribution of Asian AN transport had a negligible effect on the accumulation-mode aerosol number concentration in the Arctic during ARCTAS. Compared with background air, N-LSP was 2.3-4.7 times greater for Russian BB air but 2.4-2.6 times less for Asian AN air in both spring and summer. This result shows that the transport of Asian AN air decreases aerosol number concentrations in the Arctic, despite the large emissions of aerosols in East Asia. The very low aerosol number concentrations in Asian AN air were caused by wet removal during vertical transport in association with warm conveyor belts (WCBs). Therefore, this cleansing effect will be prominent for air transported via WCBs from other midlatitude regions and seasons. The inflow of clean midlatitude air can potentially have an important impact on accumulation-mode aerosol number concentrations in the Arctic.
C1 [Matsui, H.; Kondo, Y.; Moteki, N.; Koike, M.] Univ Tokyo, Dept Earth & Planetary Sci, Grad Sch Sci, Bunkyo Ku, Tokyo 1130033, Japan.
   [Takegawa, N.] Univ Tokyo, Adv Sci & Technol Res Ctr, Meguro Ku, Tokyo 1538904, Japan.
   [Sahu, L. K.] Phys Res Lab, Dept Space, Ahmadabad 380009, Gujarat, India.
   [Zhao, Y.] Univ Calif Davis, Air Qual Res Ctr, Davis, CA 95616 USA.
   [Fuelberg, H. E.; Sessions, W. R.] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
   [Diskin, G.; Anderson, B. E.] NASA, Chem & Dynam Branch, Langley Res Ctr, Hampton, VA 23681 USA.
   [Blake, D. R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA.
   [Wisthaler, A.] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria.
   [Cubison, M. J.; Jimenez, J. L.] Univ Colorado Boulder, CIRES, Boulder, CO 80309 USA.
   [Cubison, M. J.; Jimenez, J. L.] Univ Colorado Boulder, Dept Chem & Biochem, Boulder, CO 80309 USA.
RP Matsui, H (reprint author), Univ Tokyo, Dept Earth & Planetary Sci, Grad Sch Sci, Bunkyo Ku, Hongo 7-3-1, Tokyo 1130033, Japan.
EM matsui@eps.s.u-tokyo.ac.jp
RI Jimenez, Jose/A-5294-2008; Kondo, Yutaka/D-1459-2012; Sessions,
   Walter/O-8096-2014
OI Jimenez, Jose/0000-0001-6203-1847; Sessions, Walter/0000-0002-5376-4894
FU NASA; ARCTAS; Ministry of Education, Culture, Sports, Science, and
   Technology (MEXT); Japan Science and Technology Agency (JST); Japanese
   Ministry of the Environment [A1101]; NASA [USP-SMD-08-009, NNX08AD39G];
   Austrian Research Promotion Agency (FFG-ALR); Tiroler Zukunftstiftung
FX The ARCTAS campaign was supported by NASA. We are indebted to all the
   ARCTAS participants for their cooperation and support. Special thanks
   are due to the flight and ground crews of the NASA DC-8 aircraft. We
   thank M. Osuka for his assistance with the field measurements. This work
   was supported in part by the Ministry of Education, Culture, Sports,
   Science, and Technology (MEXT), the strategic international cooperative
   program of the Japan Science and Technology Agency (JST), and the global
   environment research fund of the Japanese Ministry of the Environment
   (A1101). Y.Z. was supported in part by NASA's Tropospheric Chemistry
   Program (USP-SMD-08-009). CH<INF>3</INF>CN measurements were supported
   by the Austrian Research Promotion Agency (FFG-ALR) and the Tiroler
   Zukunftstiftung and were carried out with the help/support of T.
   Mikoviny, M. Graus, A. Hansel, and T. D. Maerk. M.J.C. and J.L.J. were
   supported by NASA NNX08AD39G.
NR 68
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Z9 6
U1 6
U2 21
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 OCT 29
PY 2011
VL 116
AR D20217
DI 10.1029/2011JD016189
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 839AN
UT WOS:000296336800004
ER

PT J
AU Wang, JQ
   Jiang, X
   Chahine, MT
   Liang, MC
   Olsen, ET
   Chen, LL
   Licata, SJ
   Pagano, TS
   Yung, YL
AF Wang, Jingqian
   Jiang, Xun
   Chahine, Moustafa T.
   Liang, Mao-Chang
   Olsen, Edward T.
   Chen, Luke L.
   Licata, Stephen J.
   Pagano, Thomas S.
   Yung, Yuk L.
TI The influence of tropospheric biennial oscillation on mid-tropospheric
   CO2
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MONSOON RAINFALL; SUMMER MONSOON; ASIAN MONSOON; VARIABILITY; OCEAN;
   SYSTEM
AB Mid-tropospheric CO2 retrieved from the Atmospheric Infrared Sounder (AIRS) was used to investigate CO2 inter-annual variability over the Indo-Pacific region. A signal with periodicity around two years was found for the AIRS mid-tropospheric CO2 for the first time, which is related to the Tropospheric Biennial Oscillation (TBO) associated with the strength of the monsoon. During a strong (weak) monsoon year, the Western Walker Circulation is strong (weak), resulting in enhanced (diminished) CO2 transport from the surface to the mid-troposphere. As a result, there are positive (negative) CO2 anomalies at mid-troposphere over the Indo-Pacific region. We simulated the influence of the TBO on the mid-tropospheric CO2 over the Indo-Pacific region using the MOZART-2 model, and results were consistent with observations, although we found the TBO signal in the model CO2 is to be smaller than that in the AIRS observations. Citation: Wang, J., X. Jiang, M. T. Chahine, M.-C. Liang, E. T. Olsen, L. L. Chen, S. J. Licata, T. S. Pagano, and Y. L. Yung (2011), The influence of tropospheric biennial oscillation on mid-tropospheric CO2, Geophys. Res. Lett., 38, L20805, doi:10.1029/2011GL049288.
C1 [Wang, Jingqian; Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
   [Chahine, Moustafa T.; Olsen, Edward T.; Chen, Luke L.; Licata, Stephen J.; Pagano, Thomas S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Liang, Mao-Chang] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan.
   [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Liang, Mao-Chang] Natl Cent Univ, Grad Inst Astron, Jhongli, Taiwan.
RP Wang, JQ (reprint author), Univ Houston, Dept Earth & Atmospher Sci, 4800 Calhoun Rd, Houston, TX 77204 USA.
EM xjiang4@mail.uh.edu
FU JPL [G99694, P765982]
FX We specially acknowledge Alexander Ruzmaikin, Runlie Shia, Fai Li, and
   three anonymous reviewers, who gave helpful comments on this research.
   X. Jiang is supported by JPL grant G99694. Y. L. Yung is supported by
   JPL grant P765982 to the California Institute of Technology.
NR 29
TC 7
Z9 7
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 29
PY 2011
VL 38
AR L20805
DI 10.1029/2011GL049288
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 839DI
UT WOS:000296344700004
ER

PT J
AU Green, RO
   Pieters, C
   Mouroulis, P
   Eastwood, M
   Boardman, J
   Glavich, T
   Isaacson, P
   Annadurai, M
   Besse, S
   Barr, D
   Buratti, B
   Cate, D
   Chatterjee, A
   Clark, R
   Cheek, L
   Combe, J
   Dhingra, D
   Essandoh, V
   Geier, S
   Goswami, JN
   Green, R
   Haemmerle, V
   Head, J
   Hovland, L
   Hyman, S
   Klima, R
   Koch, T
   Kramer, G
   Kumar, ASK
   Lee, K
   Lundeen, S
   Malaret, E
   McCord, T
   McLaughlin, S
   Mustard, J
   Nettles, J
   Petro, N
   Plourde, K
   Racho, C
   Rodriquez, J
   Runyon, C
   Sellar, G
   Smith, C
   Sobel, H
   Staid, M
   Sunshine, J
   Taylor, L
   Thaisen, K
   Tompkins, S
   Tseng, H
   Vane, G
   Varanasi, P
   White, M
   Wilson, D
AF Green, R. O.
   Pieters, C.
   Mouroulis, P.
   Eastwood, M.
   Boardman, J.
   Glavich, T.
   Isaacson, P.
   Annadurai, M.
   Besse, S.
   Barr, D.
   Buratti, B.
   Cate, D.
   Chatterjee, A.
   Clark, R.
   Cheek, L.
   Combe, J.
   Dhingra, D.
   Essandoh, V.
   Geier, S.
   Goswami, J. N.
   Green, R.
   Haemmerle, V.
   Head, J.
   Hovland, L.
   Hyman, S.
   Klima, R.
   Koch, T.
   Kramer, G.
   Kumar, A. S. K.
   Lee, K.
   Lundeen, S.
   Malaret, E.
   McCord, T.
   McLaughlin, S.
   Mustard, J.
   Nettles, J.
   Petro, N.
   Plourde, K.
   Racho, C.
   Rodriquez, J.
   Runyon, C.
   Sellar, G.
   Smith, C.
   Sobel, H.
   Staid, M.
   Sunshine, J.
   Taylor, L.
   Thaisen, K.
   Tompkins, S.
   Tseng, H.
   Vane, G.
   Varanasi, P.
   White, M.
   Wilson, D.
TI The Moon Mineralogy Mapper (M-3) imaging spectrometer for lunar science:
   Instrument description, calibration, on-orbit measurements, science data
   calibration and on-orbit validation
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MISSION; AVIRIS; SPECTROSCOPY
AB The NASA Discovery Moon Mineralogy Mapper imaging spectrometer was selected to pursue a wide range of science objectives requiring measurement of composition at fine spatial scales over the full lunar surface. To pursue these objectives, a broad spectral range imaging spectrometer with high uniformity and high signal-to-noise ratio capable of measuring compositionally diagnostic spectral absorption features from a wide variety of known and possible lunar materials was required. For this purpose the Moon Mineralogy Mapper imaging spectrometer was designed and developed that measures the spectral range from 430 to 3000 nm with 10 nm spectral sampling through a 24 degree field of view with 0.7 milliradian spatial sampling. The instrument has a signal-to-noise ratio of greater than 400 for the specified equatorial reference radiance and greater than 100 for the polar reference radiance. The spectral cross-track uniformity is >90% and spectral instantaneous field-of-view uniformity is >90%. The Moon Mineralogy Mapper was launched on Chandrayaan-1 on the 22nd of October. On the 18th of November 2008 the Moon Mineralogy Mapper was turned on and collected a first light data set within 24 h. During this early checkout period and throughout the mission the spacecraft thermal environment and orbital parameters varied more than expected and placed operational and data quality constraints on the measurements. On the 29th of August 2009, spacecraft communication was lost. Over the course of the flight mission 1542 downlinked data sets were acquired that provide coverage of more than 95% of the lunar surface. An end-to-end science data calibration system was developed and all measurements have been passed through this system and delivered to the Planetary Data System (PDS.NASA.GOV). An extensive effort has been undertaken by the science team to validate the Moon Mineralogy Mapper science measurements in the context of the mission objectives. A focused spectral, radiometric, spatial, and uniformity validation effort has been pursued with selected data sets including an Earth-view data set. With this effort an initial validation of the on-orbit performance of the imaging spectrometer has been achieved, including validation of the cross-track spectral uniformity and spectral instantaneous field of view uniformity. The Moon Mineralogy Mapper is the first imaging spectrometer to measure a data set of this kind at the Moon. These calibrated science measurements are being used to address the full set of science goals and objectives for this mission.
C1 [Green, R. O.; Mouroulis, P.; Eastwood, M.; Glavich, T.; Barr, D.; Buratti, B.; Cate, D.; Chatterjee, A.; Essandoh, V.; Geier, S.; Green, R.; Haemmerle, V.; Hovland, L.; Hyman, S.; Koch, T.; Lee, K.; Lundeen, S.; Plourde, K.; Racho, C.; Rodriquez, J.; Sellar, G.; Sobel, H.; Tseng, H.; Vane, G.; Varanasi, P.; White, M.; Wilson, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Pieters, C.; Isaacson, P.; Cheek, L.; Dhingra, D.; Head, J.; Klima, R.; Mustard, J.; Nettles, J.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
   [Boardman, J.] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA.
   [Annadurai, M.] ISRO Satellite Ctr, Bangalore 560017, Karnataka, India.
   [Besse, S.; McLaughlin, S.; Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Clark, R.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
   [Combe, J.; Kramer, G.; McCord, T.] Bear Fight Ctr, Winthrop, WA 98862 USA.
   [Goswami, J. N.] ISRO, Phys Res Lab, Ahmadabad 380009, Gujarat, India.
   [Kramer, G.] Lunar & Planetary Inst, Houston, TX 77058 USA.
   [Kumar, A. S. K.] ISRO, Ctr Space Applicat, Ahmadabad 380015, Gujarat, India.
   [Malaret, E.] Appl Coherent Technol, Herndon, VA USA.
   [Petro, N.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA.
   [Runyon, C.] Coll Charleston, Dept Geol & Environm Geosci, Charleston, SC 29424 USA.
   [Smith, C.] ATK, Pasadena, CA 91107 USA.
   [Staid, M.] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [Taylor, L.; Thaisen, K.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA.
   [Tompkins, S.] DARPA, Arlington, VA 22203 USA.
RP Green, RO (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.o.green@jpl.nasa.gov
RI Klima, Rachel/H-9383-2012; Petro, Noah/F-5340-2013; 
OI Klima, Rachel/0000-0002-9151-6429; Besse, Sebastien/0000-0002-1052-5439
FU National Aeronautics and Space Administration
FX The authors are deeply grateful to the Indian Space Research
   Organization for providing this guest opportunity for M<SUP>3</SUP> to
   participate in the Chandrayaan-1 mission and the broad support over the
   course of the mission including contributions for this paper. We also
   gratefully acknowledge the NASA Discovery Program for supporting
   M<SUP>3</SUP> development, implementation and science validation. A
   portion of this work was carried out at the Jet Propulsion
   Laboratory/California Institute of Technology, Pasadena, California,
   under contract with the National Aeronautics and Space Administration.
NR 33
TC 61
Z9 61
U1 1
U2 21
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 OCT 29
PY 2011
VL 116
AR E00G19
DI 10.1029/2011JE003797
PG 31
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 839AQ
UT WOS:000296337200001
ER

PT J
AU Zhang, ZB
   Platnick, S
AF Zhang, Zhibo
   Platnick, Steven
TI An assessment of differences between cloud effective particle radius
   retrievals for marine water clouds from three MODIS spectral bands
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DROPLET EFFECTIVE RADIUS; REMOTE-SENSING PROBLEMS; STRATOCUMULUS CLOUDS;
   STRATIFORM CLOUDS; PHOTON TRANSPORT; MICROPHYSICS; GROWTH; ENTRAINMENT;
   VARIABILITY; EVOLUTION
AB The Moderate Resolution Imaging Spectroradiometer (MODIS) cloud product provides three separate 1 km resolution retrievals of cloud particle effective radii (r(e)), derived from 1.6, 2.1 and 3.7 mu m band observations. In this study, differences among the three size retrievals for maritime water clouds (designated as r(e,1.6) r(e,2.1) and r(e,3.7)) were systematically investigated through a series of case studies and global analyses. Substantial differences are found between r(e,3.7) and r(e,2.1) retrievals (Delta r(e,3.7-2.1)), with a strong dependence on cloud regime. The differences are typically small, within +/- 2 mu m, over relatively spatially homogeneous costal stratocumulus cloud regions. However, for trade wind cumulus regimes, r(e,3.7) was found to be substantially smaller than r(e,2.1), sometimes by more than 10 mu m. The correlation of Delta r(e,3.7-2.1) with key cloud parameters, including the cloud optical thickness (tau), r(e) and a cloud horizontal heterogeneity index (H-sigma) derived from 250m resolution MODIS 0.86 mu m band observations, were investigated using one month of MODIS Terra data. It was found that differences among the three r(e) retrievals for optically thin clouds (tau < 5) are highly variable, ranging from -15 mu m to 10 mu m, likely due to the large MODIS retrieval uncertainties when the cloud is thin. The Delta r(e),(3.7-2.1) exhibited a threshold-like dependence on both r(e,2.1) and H-sigma. The r(e,3.7) is found to agree reasonably well with re,(2.1) when r(e,2.1) is smaller than about 15 mu m, but becomes increasingly smaller than r(e,2.1) once r(e,2.1) exceeds this size. All three r(e) retrievals showed little dependence when cloud is relatively homogenous (H-sigma < 0.3 defined as standard deviation divided by the mean for the 250 m pixels within a 1 km pixel retrieval). However, for inhomogeneous clouds (H-sigma > 0.3), both r(e, 1.6) and r(e,2.1) were seen to increase quickly with H-sigma. On the other hand, r(e,3.7) statistics showed little dependence on H-sigma and remained relatively stable over the whole range of H-sigma values. Potential contributing causes to the substantial r(e,3.7) and r(e,2.1) differences are discussed. In particular, based on both 1-D and 3-D radiative transfer simulations, we have elucidated mechanisms by which cloud heterogeneity and 3-D radiative effects can cause large differences between r(e,3.7) and r(e,2.1) retrievals for highly inhomogeneous clouds. Our results suggest that the contrast in observed Delta r(e,3.7-2.1) between cloud regimes is correlated with increases in both cloud re and Hs. We also speculate that in some highly inhomogeneous drizzling clouds, vertical structure induced by drizzle and 3-D radiative effects might operate together to cause dramatic differences between r(e,3.7) and r(e,2.1) retrievals.
C1 [Zhang, Zhibo] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 20723 USA.
   [Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 20723 USA.
   [Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhang, ZB (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 20723 USA.
EM Zhibo.Zhang@umbc.edu
RI Zhang, Zhibo/D-1710-2010; Platnick, Steven/J-9982-2014
OI Zhang, Zhibo/0000-0001-9491-1654; Platnick, Steven/0000-0003-3964-3567
FU NASA [NNX11AI98G]
FX We would like to thank Brent Maddux and Steve Ackerman for many helpful
   discussions. We also thank Gala Wind for providing research-level MOD06
   code and Kerry Meyer for proofreading the manuscript and providing
   helpful suggestions. Z.Z. acknowledges NASA funding support under the
   grant NNX11AI98G. Z.Z. would like to thank Alexander Marshak and Tamas
   Varnai for valuable discussion on 3-D radiative effect, and Robert
   Pincus for his help on I3RC code. This work was funded in part by NASA's
   Radiation Sciences Program.
NR 51
TC 70
Z9 70
U1 3
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 28
PY 2011
VL 116
AR D20215
DI 10.1029/2011JD016216
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 839AM
UT WOS:000296336700006
ER

PT J
AU Sparks, L
   Blanch, J
   Pandya, N
AF Sparks, Lawrence
   Blanch, Juan
   Pandya, Nitin
TI Estimating ionospheric delay using kriging: 2. Impact on satellite-based
   augmentation system availability
SO RADIO SCIENCE
LA English
DT Article
AB An augmentation of the Global Positioning System, the Wide Area Augmentation System (WAAS) broadcasts, at each node of an ionospheric grid, an estimate of the vertical ionospheric delay and an integrity bound on the vertical delay error. To date, these quantities have been determined from a planar fit of slant delay measurements, projected to vertical using an obliquity factor specified by the standard thin shell model of the ionosphere. In a future WAAS upgrade (WAAS Follow-On Release 3), however, they will be calculated using an established, geo-statistical estimation technique known as kriging that generally provides higher estimate accuracy than planar fit estimation. This paper analyzes the impact of kriging on system availability. In a preliminary assessment, kriging is found to produce improvements in availability of up to 15%.
C1 [Sparks, Lawrence] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Blanch, Juan] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
   [Pandya, Nitin] Raytheon Co, Fullerton, CA 92833 USA.
RP Sparks, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sparks@jpl.nasa.gov
NR 13
TC 15
Z9 15
U1 2
U2 7
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 OCT 28
PY 2011
VL 46
AR RS0D22
DI 10.1029/2011RS004781
PG 10
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences; Remote Sensing; Telecommunications
GA 839HM
UT WOS:000296356100001
ER

PT J
AU Davami, K
   Ghassemi, HM
   Sun, XH
   Yassar, RS
   Lee, JS
   Meyyappan, M
AF Davami, Keivan
   Ghassemi, Hessam M.
   Sun, Xuhui
   Yassar, Reza S.
   Lee, Jeong-Soo
   Meyyappan, M.
TI In situ observation of morphological change in CdTe nano- and submicron
   wires
SO NANOTECHNOLOGY
LA English
DT Article
ID NANOWIRES; TRANSPORT; ARRAYS
AB We report growth and characterization of CdTe wires 30-400 nm in diameter by the vapor-liquid-solid technique. Individual nanowires were placed on a movable piezotube, which allowed three-dimensional motion toward a scanning tunneling microscope (STM). A bias was applied to the STM tip in contact with the nanowire, and the morphological changes due to Joule heating were observed in situ using a transmission electron microscope (TEM) in real time. For thick CdTe wires (d > similar to 150 nm), the process results in the growth of superfine nanowires (SFNWs) of 2-4 nm diameter on the surface of the wire. Smaller diameter nanowires, in contrast, disintegrate under the applied bias before the complete evolution of SFNWs on the surface.
C1 [Davami, Keivan; Lee, Jeong-Soo; Meyyappan, M.] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang, South Korea.
   [Ghassemi, Hessam M.; Yassar, Reza S.] Michigan Technol Univ, Dept Mech Engn, Houghton, MI 49931 USA.
   [Sun, Xuhui] Soochow Univ, Inst Funct Nano & Soft Mat FUNSOM, Suzhou 215123, Jiangsu, Peoples R China.
   [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Davami, K (reprint author), Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang, South Korea.
EM ljs6951@postech.ac.kr; m.meyyappan@nasa.gov
RI Sun, Xuhui /K-5689-2012
FU World Class University through National Research Foundation of Korea;
   Ministry of Education, Science and Technology [R31-2008-000-10100-0];
   NSF-DMR [0820884]; NSF-CMMI [0926819]
FX This work was supported by the World Class University program through
   the National Research Foundation of Korea funded by the Ministry of
   Education, Science and Technology under project R31-2008-000-10100-0.
   Part of this work was done at MTU during KD's visit and Professor
   Yassar's group is acknowledged for hosting the visit.; RSY would like to
   acknowledge the funding support through the NSF-DMR grant 0820884 and
   NSF-CMMI grant 0926819. The authors thank Professor Mahendra Sunkara for
   many valuable discussions.
NR 23
TC 6
Z9 6
U1 3
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD OCT 28
PY 2011
VL 22
IS 43
AR 435204
DI 10.1088/0957-4484/22/43/435204
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
   Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 834NW
UT WOS:000295969600005
PM 21971180
ER

PT J
AU Patzold, M
   Andert, TP
   Asmar, SW
   Anderson, JD
   Barriot, JP
   Bird, MK
   Hausler, B
   Hahn, M
   Tellmann, S
   Sierks, H
   Lamy, P
   Weiss, BP
AF Paetzold, M.
   Andert, T. P.
   Asmar, S. W.
   Anderson, J. D.
   Barriot, J. -P.
   Bird, M. K.
   Haeusler, B.
   Hahn, M.
   Tellmann, S.
   Sierks, H.
   Lamy, P.
   Weiss, B. P.
TI Asteroid 21 Lutetia: Low Mass, High Density
SO SCIENCE
LA English
DT Article
AB Asteroid 21 Lutetia was approached by the Rosetta spacecraft on 10 July 2010. The additional Doppler shift of the spacecraft radio signals imposed by 21 Lutetia's gravitational perturbation on the flyby trajectory were used to determine the mass of the asteroid. Calibrating and correcting for all Doppler contributions not associated with Lutetia, a least-squares fit to the residual frequency observations from 4 hours before to 6 hours after closest approach yields a mass of (1.700 +/- 0.017) x 10(18) kilograms. Using the volume model of Lutetia determined by the Rosetta Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) camera, the bulk density, an important parameter for clues to its composition and interior, is (3.4 +/- 0.3) x 10(3) kilograms per cubic meter.
C1 [Paetzold, M.; Bird, M. K.; Hahn, M.; Tellmann, S.] Univ Cologne, Abt Planetenforsch, Rhein Inst Umweltforsch, D-50931 Cologne, Germany.
   [Andert, T. P.; Haeusler, B.] Univ Bundeswehr Munchen, Inst Raumfahrttech, D-85579 Neubiberg, Germany.
   [Asmar, S. W.; Anderson, J. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Barriot, J. -P.] Univ Polynesie Francaise, Faaa 98702, Tahiti, Fr Polynesia.
   [Bird, M. K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
   [Sierks, H.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
   [Lamy, P.] Lab Astrophys Marseille, Marseille, France.
   [Weiss, B. P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Patzold, M (reprint author), Univ Cologne, Abt Planetenforsch, Rhein Inst Umweltforsch, D-50931 Cologne, Germany.
EM martin.paetzold@uni-koeln.de
FU Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Bonn [50QM1002,
   50QM1004]; NASA
FX The Rosetta Radio Science Investigation experiment is funded by the
   Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Bonn under grants
   50QM1002 (T.P.A. and B.H.) and 50QM1004 (M.P., M.H., S.T., and M.K.B.),
   and under a contract with NASA (S.W.A. and J.D.A.). We thank T. Morley
   for valuable comments and all persons involved in Rosetta at the
   European Space Research and Technology Centre, European Space Operations
   Centre, European Space Astronomy Centre, Jet Propulsion Laboratory, and
   the European Space Tracking Network and Deep Space Network ground
   stations for their continuous support.
NR 5
TC 36
Z9 36
U1 0
U2 1
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 OCT 28
PY 2011
VL 334
IS 6055
BP 491
EP 492
DI 10.1126/science.1209389
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 837UR
UT WOS:000296230500040
PM 22034429
ER

PT J
AU Coradini, A
   Capaccioni, F
   Erard, S
   Arnold, G
   De Sanctis, MC
   Filacchione, G
   Tosi, F
   Barucci, MA
   Capria, MT
   Ammannito, E
   Grassi, D
   Piccioni, G
   Giuppi, S
   Bellucci, G
   Benkhoff, J
   Bibring, JP
   Blanco, A
   Blecka, M
   Bockelee-Morvan, D
   Carraro, F
   Carlson, R
   Carsenty, U
   Cerroni, P
   Colangeli, L
   Combes, M
   Combi, M
   Crovisier, J
   Drossart, P
   Encrenaz, ET
   Federico, C
   Fink, U
   Fonti, S
   Giacomini, L
   Ip, WH
   Jaumann, R
   Kuehrt, E
   Langevin, Y
   Magni, G
   McCord, T
   Mennella, V
   Mottola, S
   Neukum, G
   Orofino, V
   Palumbo, P
   Schade, U
   Schmitt, B
   Taylor, F
   Tiphene, D
   Tozzi, G
AF Coradini, A.
   Capaccioni, F.
   Erard, S.
   Arnold, G.
   De Sanctis, M. C.
   Filacchione, G.
   Tosi, F.
   Barucci, M. A.
   Capria, M. T.
   Ammannito, E.
   Grassi, D.
   Piccioni, G.
   Giuppi, S.
   Bellucci, G.
   Benkhoff, J.
   Bibring, J. P.
   Blanco, A.
   Blecka, M.
   Bockelee-Morvan, D.
   Carraro, F.
   Carlson, R.
   Carsenty, U.
   Cerroni, P.
   Colangeli, L.
   Combes, M.
   Combi, M.
   Crovisier, J.
   Drossart, P.
   Encrenaz, E. T.
   Federico, C.
   Fink, U.
   Fonti, S.
   Giacomini, L.
   Ip, W. H.
   Jaumann, R.
   Kuehrt, E.
   Langevin, Y.
   Magni, G.
   McCord, T.
   Mennella, V.
   Mottola, S.
   Neukum, G.
   Orofino, V.
   Palumbo, P.
   Schade, U.
   Schmitt, B.
   Taylor, F.
   Tiphene, D.
   Tozzi, G.
TI The Surface Composition and Temperature of Asteroid 21 Lutetia As
   Observed by Rosetta/VIRTIS
SO SCIENCE
LA English
DT Article
ID NEAR-INFRARED SPECTROSCOPY; FLY-BY; ALBEDO; CHONDRITES; SPECTRA;
   MISSION; BELT; SIZE
AB The Visible, InfraRed, and Thermal Imaging Spectrometer (VIRTIS) on Rosetta obtained hyperspectral images, spectral reflectance maps, and temperature maps of the asteroid 21 Lutetia. No absorption features, of either silicates or hydrated minerals, have been detected across the observed area in the spectral range from 0.4 to 3.5 micrometers. The surface temperature reaches a maximum value of 245 kelvin and correlates well with topographic features. The thermal inertia is in the range from 20 to 30 joules meter(-2) kelvin(-1) second(-0.5), comparable to a lunarlike powdery regolith. Spectral signatures of surface alteration, resulting from space weathering, seem to be missing. Lutetia is likely a remnant of the primordial planetesimal population, unaltered by differentiation processes and composed of chondritic materials of enstatitic or carbonaceous origin, dominated by iron-poor minerals that have not suffered aqueous alteration.
C1 [Capaccioni, F.; De Sanctis, M. C.; Filacchione, G.; Capria, M. T.; Piccioni, G.; Cerroni, P.; Magni, G.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
   [Coradini, A.; Tosi, F.; Ammannito, E.; Grassi, D.; Giuppi, S.; Bellucci, G.; Carraro, F.; Giacomini, L.] Inst Nazl Astrofis INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy.
   [Erard, S.; Barucci, M. A.; Bockelee-Morvan, D.; Combes, M.; Crovisier, J.; Drossart, P.; Encrenaz, E. T.; Tiphene, D.] Univ Paris Diderot, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92195 Meudon, France.
   [Arnold, G.] Inst Planetol, D-48149 Munster, Germany.
   [Benkhoff, J.; Colangeli, L.] European Space Agcy, European Space Res & Technol Ctr ESTEC, NL-2200 AG Noordwijk, Netherlands.
   [Bibring, J. P.; Langevin, Y.] CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
   [Blecka, M.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland.
   [Carlson, R.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Carsenty, U.; Jaumann, R.; Kuehrt, E.; Mottola, S.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetary Res, D-12489 Berlin, Germany.
   [Combi, M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
   [Federico, C.] Univ Perugia, I-06100 Perugia, Italy.
   [Fink, U.] Univ Arizona, Lunar Planetary Lab, Tucson, AZ 85721 USA.
   [Blanco, A.; Fonti, S.; Orofino, V.] Univ Lecce, Dipartimento Fis, I-73100 Lecce, Italy.
   [Ip, W. H.] Natl Cent Univ, Taipei, Taiwan.
   [McCord, T.] Bear Fight Inst, Winthrop, WA 98862 USA.
   [Neukum, G.] Free Univ Berlin, D-14195 Berlin, Germany.
   [Schmitt, B.] Univ Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France.
   [Tozzi, G.] Osserv Astrofis Arcetri, I-50125 Florence, Italy.
   [Mennella, V.] Osservatorio Capodimonte, I-80131 Naples, Italy.
   [Taylor, F.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England.
   [Palumbo, P.] Univ Napoli Parthenope, I-80133 Naples, Italy.
   [Schade, U.] Helmholtz Zentrum Berlin Mat & Energie, D-14109 Berlin, Germany.
RP Capaccioni, F (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
EM fabrizio.capaccioni@inaf.it
RI Schmitt, Bernard/A-1064-2009; Combi, Michael/J-1697-2012; Schade,
   Ulrich/D-9341-2013; De Sanctis, Maria Cristina/G-5232-2013; 
OI Tozzi, Gian Paolo/0000-0003-4775-5788; Tosi,
   Federico/0000-0003-4002-2434; Schmitt, Bernard/0000-0002-1230-6627;
   Combi, Michael/0000-0002-9805-0078; Grassi, Davide/0000-0003-1653-3066;
   De Sanctis, Maria Cristina/0000-0002-3463-4437; Cerroni,
   Priscilla/0000-0003-0239-2741; Bellucci, Giancarlo/0000-0003-0867-8679;
   Capaccioni, Fabrizio/0000-0003-1631-4314; Filacchione,
   Gianrico/0000-0001-9567-0055; Piccioni, Giuseppe/0000-0002-7893-6808
FU Rosetta Science Operations Centre; Rosetta Mission Operations Centre;
   Agenzia Spaziale Italiana; Centre National d'Etudes Spatiales; Deutsches
   Zentrum fur Luft- und Raumfahrt
FX The authors wish to thank L. V. Moroz for helpful comments during the
   revision phase and the Rosetta Science Operations Centre and the Rosetta
   Mission Operations Centre for their support. VIRTIS was built by a
   European consortium and is part of the Rosetta spacecraft, provided by
   the European Space Agency (ESA). We acknowledge the funding of the
   national space agencies: Agenzia Spaziale Italiana, Centre National
   d'Etudes Spatiales, Deutsches Zentrum fur Luft- und Raumfahrt. The
   VIRTIS calibrated data will be available through the ESA's Planetary
   Science Archive (PSA) Web site
   (www.rssd.esa.int/index.php?project=PSA&page=index) in 2011.
NR 32
TC 50
Z9 51
U1 0
U2 13
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 OCT 28
PY 2011
VL 334
IS 6055
BP 492
EP 494
DI 10.1126/science.1204062
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 837UR
UT WOS:000296230500041
PM 22034430
ER

PT J
AU Fox, N
   Kaiser-Weiss, A
   Schmutz, W
   Thome, K
   Young, D
   Wielicki, B
   Winkler, R
   Woolliams, E
AF Fox, Nigel
   Kaiser-Weiss, Andrea
   Schmutz, Werner
   Thome, Kurtis
   Young, Dave
   Wielicki, Bruce
   Winkler, Rainer
   Woolliams, Emma
TI Accurate radiometry from space: an essential tool for climate studies
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
   AND ENGINEERING SCIENCES
LA English
DT Article
DE climate change; Earth observation; satellites; radiometry; solar
   irradiance
ID SPECTRAL IRRADIANCE; CRYOGENIC-RADIOMETER; THERMODYNAMIC TEMPERATURES;
   RESPONSIVITY CALIBRATIONS; SOLAR; SCALE; UNCERTAINTY; REQUIREMENTS;
   VARIABILITY; PHOTODIODES
AB The Earth's climate is undoubtedly changing; however, the time scale, consequences and causal attribution remain the subject of significant debate and uncertainty. Detection of subtle indicators from a background of natural variability requires measurements over a time base of decades. This places severe demands on the instrumentation used, requiring measurements of sufficient accuracy and sensitivity that can allow reliable judgements to be made decades apart. The International System of Units ( SI) and the network of National Metrology Institutes were developed to address such requirements. However, ensuring and maintaining SI traceability of sufficient accuracy in instruments orbiting the Earth presents a significant new challenge to the metrology community. This paper highlights some key measurands and applications driving the uncertainty demand of the climate community in the solar reflective domain, e. g. solar irradiances and reflectances/radiances of the Earth. It discusses how meeting these uncertainties facilitate significant improvement in the forecasting abilities of climate models. After discussing the current state of the art, it describes a new satellite mission, called TRUTHS, which enables, for the first time, high-accuracy SI traceability to be established in orbit. The direct use of a 'primary standard' and replication of the terrestrial traceability chain extends the SI into space, in effect realizing a 'metrology laboratory in space'.
C1 [Fox, Nigel; Winkler, Rainer; Woolliams, Emma] Natl Phys Lab, Teddington TW11 0LW, Middx, England.
   [Kaiser-Weiss, Andrea] Univ Reading, Natl Ctr Earth Observat, Reading RG6 6BB, Berks, England.
   [Schmutz, Werner] Phys Meteorol Observ Davos, World Radiat Ctr, CH-7260 Davos, Switzerland.
   [Thome, Kurtis] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Young, Dave; Wielicki, Bruce] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Fox, N (reprint author), Natl Phys Lab, Hampton Rd, Teddington TW11 0LW, Middx, England.
EM nigel.fox@npl.co.uk
RI Thome, Kurtis/D-7251-2012; Woolliams, Emma/A-2404-2014; Schmutz,
   Werner/B-4153-2014
OI Woolliams, Emma/0000-0003-3517-1486; Schmutz, Werner/0000-0003-1159-5639
FU National Measurement Office of the BIS Department of the UK
FX The authors would like to acknowledge the support and contributions of
   the following individuals (alphabetical by host institute) and
   organizations to the TRUTHS mission concept, which is in part summarized
   by this paper: T. Quinn FRS (BIPM), G. Myhre (CICERO, Norway), P. Henry
   (CNES, France), R. Bantges, R. Brindley, J. Haigh and J. Russell
   (Imperial College London, UK), M. Verstraate and J.-L. Widlowski
   (JRC-Ispra, EC), J.-P. Muller (MSSL, UK), A. Shaw (NCEO, UK), X.
   Briottet (ONERA, France), S. Groom (Plymouth Marine Laboratory, UK), S.
   Mackin (SSTL, UK), R. Saunders (UK Meteorological Office), P. Teillet
   (University of Lethbridge, Canada), R. Allen and K. Shine FRS
   (University of Reading, UK), M. Schaepman (University of Zurich,
   Switzerland), G. Stensaas and T. Stone (USGS, USA), EADS Astrium UK, OIP
   Belgium, Serco, Italy, SSTL UK and STFC (RAL) UK. In addition, Nigel Fox
   would like to thank the National Measurement Office of the BIS
   Department of the UK for financial support to this work.
NR 65
TC 27
Z9 31
U1 1
U2 13
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
EI 1471-2962
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD OCT 28
PY 2011
VL 369
IS 1953
BP 4028
EP 4063
DI 10.1098/rsta.2011.0246
PG 36
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 821SJ
UT WOS:000294994400010
PM 21930564
ER

PT J
AU Rosenfeld, D
   Bell, TL
AF Rosenfeld, Daniel
   Bell, Thomas L.
TI Why do tornados and hailstorms rest on weekends?
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DEEP CONVECTIVE CLOUDS; UNITED-STATES; AEROSOL IMPACTS; CUMULUS CLOUD;
   AMAZON; STORMS; PRECIPITATION; MICROPHYSICS; THUNDERSTORM; POLLUTION
AB This study shows for the first time statistical evidence that when anthropogenic aerosols over the eastern United States during summertime are at their weekly mid-week peak, tornado and hailstorm activity there is also near its weekly maximum. The weekly cycle in summertime storm activity for 1995-2009 was found to be statistically significant and unlikely to be due to natural variability. It correlates well with previously observed weekly cycles of other measures of storm activity. The pattern of variability supports the hypothesis that air pollution aerosols invigorate deep convective clouds in a moist, unstable atmosphere, to the extent of inducing production of large hailstones and tornados. This is caused by the effect of aerosols on cloud drop nucleation, making cloud drops smaller and hydrometeors larger. According to simulations, the larger ice hydrometeors contribute to more hail. The reduced evaporation from the larger hydrometeors produces weaker cold pools. Simulations have shown that too cold and fast-expanding pools inhibit the formation of tornados. The statistical observations suggest that this might be the mechanism by which the weekly modulation in pollution aerosols is causing the weekly cycle in severe convective storms during summer over the eastern United States. Although we focus here on the role of aerosols, they are not a primary atmospheric driver of tornados and hailstorms but rather modulate them in certain conditions.
C1 [Rosenfeld, Daniel] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
   [Bell, Thomas L.] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA.
RP Rosenfeld, D (reprint author), Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
EM daniel.rosenfeld@huji.ac.il
RI Bell, Thomas/G-5425-2012; Rosenfeld, Daniel/F-6077-2016
OI Rosenfeld, Daniel/0000-0002-0784-7656
FU European Community-New and Emerging Science and Technologies [12444];
   Science Mission Directorate of NASA
FX We thank Greg Carbin (NOAA/NWS) for his help in understanding the severe
   storms data set. We also thank Earle Williams for many helpful comments
   on the manuscript. Research by D.R. is an outcome of the European
   Community-New and Emerging Science and Technologies (contract 12444
   NEST-ANTISTORM). Research by T.L.B. was supported by the Science Mission
   Directorate of NASA as part of the Precipitation Measurement Mission
   program under Ramesh Kakar.
NR 60
TC 28
Z9 28
U1 0
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 27
PY 2011
VL 116
AR D20211
DI 10.1029/2011JD016214
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 839AK
UT WOS:000296336500003
ER

PT J
AU Smith, DM
   Dwyer, JR
   Hazelton, BJ
   Grefenstette, BW
   Martinez-McKinney, GFM
   Zhang, ZY
   Lowell, AW
   Kelley, NA
   Splitt, ME
   Lazarus, SM
   Ulrich, W
   Schaal, M
   Saleh, ZH
   Cramer, E
   Rassoul, H
   Cummer, SA
   Lu, G
   Shao, XM
   Ho, C
   Hamlin, T
   Blakeslee, RJ
   Heckman, S
AF Smith, D. M.
   Dwyer, J. R.
   Hazelton, B. J.
   Grefenstette, B. W.
   Martinez-McKinney, G. F. M.
   Zhang, Z. Y.
   Lowell, A. W.
   Kelley, N. A.
   Splitt, M. E.
   Lazarus, S. M.
   Ulrich, W.
   Schaal, M.
   Saleh, Z. H.
   Cramer, E.
   Rassoul, H.
   Cummer, S. A.
   Lu, G.
   Shao, X. -M.
   Ho, C.
   Hamlin, T.
   Blakeslee, R. J.
   Heckman, S.
TI A terrestrial gamma ray flash observed from an aircraft
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID X-RAYS; THUNDERSTORM
AB On 21 August 2009, the Airborne Detector for Energetic Lightning Emissions (ADELE), an array of six gamma-ray detectors, detected a brief burst of gamma rays while flying aboard a Gulfstream V jet near two active thunderstorm cells. The duration and spectral characteristics of the event are consistent with the terrestrial gamma ray flashes (TGFs) seen by instruments in low Earth orbit. A long-duration, complex +IC flash was taking place in the nearer cell at the same time, at a distance of similar to 10 km from the plane. The sferics that are probably associated with this flash extended over 54 ms and included several ULF pulses corresponding to charge moment changes of up to 30 C km, this value being in the lower half of the range of sferics associated with TGFs seen from space. Monte Carlo simulations of gamma ray propagation in the Earth's atmosphere show that a TGF of normal intensity would, at this distance, have produced a gamma ray signal in ADELE of approximately the size and spectrum that was actually observed. We conclude that this was the first detection of a TGF from an aircraft. We show that because of the distance, ADELE's directional and spectral capabilities could not strongly constrain the source altitude of the TGF but that such constraints would be possible for TGFs detected at closer range.
C1 [Smith, D. M.; Martinez-McKinney, G. F. M.; Zhang, Z. Y.; Kelley, N. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
   [Smith, D. M.; Lowell, A. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Dwyer, J. R.; Schaal, M.; Cramer, E.; Rassoul, H.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
   [Hazelton, B. J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
   [Grefenstette, B. W.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
   [Splitt, M. E.; Lazarus, S. M.] Florida Inst Technol, Dept Marine & Environm Syst, Melbourne, FL 32901 USA.
   [Ulrich, W.] Natl Weather Serv, Key West, FL USA.
   [Saleh, Z. H.] Mem Sloan Kettering Canc Ctr, Dept Med Phys, New York, NY 10021 USA.
   [Cummer, S. A.; Lu, G.] Duke Univ, Dept Elect & Comp Engn, Durham, NC USA.
   [Shao, X. -M.; Ho, C.; Hamlin, T.] Los Alamos Natl Lab, Los Alamos, NM USA.
   [Blakeslee, R. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
   [Heckman, S.] AWS Convergence Technol Inc, Germantown, MD USA.
RP Smith, DM (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008; 
OI Cummer, Steven/0000-0002-0002-0613; Splitt, Michael/0000-0002-7690-5100;
   Rassoul, Hamid Kyan Sam/0000-0003-0681-7276; Lazarus,
   Steven/0000-0002-5918-1059
FU NSF [ATM-0619941, ATM-0846609]
FX We thank Allen Schanot, the managing scientist of our field campaign
   from NCAR/EOL; the other NCAR scientists who filled this role earlier or
   helped us with GV data, Pavel Romashkin, Jorgen Jensen, and Jeff Stith;
   and the EOL pilots, engineers, and technicians who provided exemplary
   support. ADELE's construction was funded by NSF major research
   instrumentation grant ATM-0619941. Our simulation work was supported by
   NSF grant ATM-0846609. This work includes publicly available data from
   the KJAX NEXRAD radar of the National Weather Service.
NR 31
TC 16
Z9 16
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 27
PY 2011
VL 116
AR D20124
DI 10.1029/2011JD016252
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 839AK
UT WOS:000296336500004
ER

PT J
AU Sparks, L
   Blanch, J
   Pandya, N
AF Sparks, Lawrence
   Blanch, Juan
   Pandya, Nitin
TI Estimating ionospheric delay using kriging: 1. Methodology
SO RADIO SCIENCE
LA English
DT Article
AB The Wide Area Augmentation System (WAAS) is an augmentation of the Global Positioning System (GPS) that provides safe and reliable use of GPS signals for airline navigation over much of North America. Ever since WAAS was first commissioned in July of 2003, the vertical delay estimate at each node in the WAAS ionospheric grid has been determined from a planar fit of slant delay measurements, projected to vertical using an obliquity factor specified by the standard thin shell model of the ionosphere. In a future WAAS upgrade (WAAS Follow-On Release 3), however, the vertical delay will be estimated by an established, geo-statistical technique known as kriging. When compared to the planar fit model, the kriging model is generally found to match better the observed random structure of the vertical delay. This paper presents the kriging methodology to be used to estimate the vertical delay and its uncertainty at each ionospheric grid point. In addition, it provides examples of the improvement in delay accuracy achieved. Under disturbed conditions, the implementation of kriging reduces the magnitude of the root mean square fit residual by up to 15%.
C1 [Sparks, Lawrence] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Blanch, Juan] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
   [Pandya, Nitin] Raytheon Co, Fullerton, CA 92833 USA.
RP Sparks, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sparks@jpl.nasa.gov
FU National Aeronautics and Space Administration; Federal Aviation
   Administration
FX The research of Lawrence Sparks was performed at the Jet Propulsion
   Laboratory/California Institute of Technology under contract to the
   National Aeronautics and Space Administration and the Federal Aviation
   Administration.
NR 15
TC 18
Z9 18
U1 0
U2 2
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 OCT 27
PY 2011
VL 46
AR RS0D21
DI 10.1029/2011RS004667
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 839HL
UT WOS:000296356000001
ER

PT J
AU Kurtz, NT
   Farrell, SL
AF Kurtz, Nathan T.
   Farrell, Sinead L.
TI Large-scale surveys of snow depth on Arctic sea ice from Operation
   IceBridge
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID RADAR MEASUREMENTS; LASER ALTIMETRY; THICKNESS; REDISTRIBUTION;
   VARIABILITY; MISSION; OCEAN; LAND
AB We show the first results of a large-scale survey of snow depth on Arctic sea ice from NASA's Operation IceBridge snow radar system for the 2009 season and compare the data to climatological snow depth values established over the 1954-1991 time period. For multiyear ice, the mean radar derived snow depth is 33.1 cm and the corresponding mean climatological snow depth is 33.4 cm. The small mean difference suggests consistency between contemporary estimates of snow depth with the historical climatology for the multiyear ice region of the Arctic. A 16.5 cm mean difference (climatology minus radar) is observed for first year ice areas suggesting that the increasingly seasonal sea ice cover of the Arctic Ocean has led to an overall loss of snow as the region has transitioned away from a dominantly multiyear ice cover. Citation: Kurtz, N. T., and S. L. Farrell (2011), Large-scale surveys of snow depth on Arctic sea ice from Operation IceBridge, Geophys. Res. Lett., 38, L20505, doi: 10.1029/2011GL049216.
C1 [Kurtz, Nathan T.] Morgan State Univ, Sch Comp Math & Nat Sci, Baltimore, MD 21239 USA.
   [Kurtz, Nathan T.; Farrell, Sinead L.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
   [Farrell, Sinead L.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
RP Kurtz, NT (reprint author), Morgan State Univ, Sch Comp Math & Nat Sci, Baltimore, MD 21239 USA.
EM nathan.t.kurtz@nasa.gov
RI Farrell, Sinead/F-5586-2010
OI Farrell, Sinead/0000-0003-3222-2751
FU NASA [NNX10AV07G]; NOAA/STAR
FX This work was supported by the NASA Cryospheric Sciences Program under
   grant NNX10AV07G and the NOAA/STAR Ocean Remote Sensing Program. The
   authors would like to thank the editor and reviewers for their helpful
   suggestions on improving the manuscript.
NR 31
TC 36
Z9 38
U1 0
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 27
PY 2011
VL 38
AR L20505
DI 10.1029/2011GL049216
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 839CZ
UT WOS:000296343700004
ER

PT J
AU Gallegos, CL
   Werdell, PJ
   McClain, CR
AF Gallegos, Charles L.
   Werdell, P. Jeremy
   McClain, Charles R.
TI Long-term changes in light scattering in Chesapeake Bay inferred from
   Secchi depth, light attenuation, and remote sensing measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID EXOPOLYMER PARTICLES TEP; INHERENT OPTICAL-PROPERTIES; DISSOLVED
   ORGANIC-MATTER; INFRARED SPECTRAL REGION; OCEANIC WATERS; MARINE
   PARTICLES; COASTAL WATERS; ABSORPTION-COEFFICIENTS; NATURAL
   PHYTOPLANKTON; BACKSCATTERING RATIO
AB The relationship between the Secchi depth (Z(SD)) and the diffuse attenuation coefficient for photosynthetically active radiation (K-d(PAR)), and in particular the product of the two, Z(SD)center dot K-d(PAR), is governed primarily by the ratio of light scattering to absorption. We analyzed measurements of Z(SD) and K-d(PAR) at main stem stations in Chesapeake Bay and found that the Z(SD)center dot K-d(PAR) product has declined at rates varying from 0.020 to 0.033 yr(-1) over the 17 to 25 years of measurement, implying that there has been a long-term increase in the scattering-to-absorption ratio. Remote sensing reflectance at the green wavelength most relevant to Z(SD) and K-d(PAR) in these waters, R-rs(555), did not exhibit an increasing trend over the 10 years of available measurements. To reconcile the observations we constructed a bio-optical model to calculate Z(SD), K-d(PAR), Z(SD)center dot K-d(PAR), and R-rs(555) as a function of light attenuating substances and their mass-specific absorption and scattering coefficients. When simulations were based exclusively on changes in concentrations of light attenuating substances, a declining trend in Z(SD)center dot K-d entailed an increasing trend in R-rs(555), contrary to observations. To simulate both decreasing Z(SD center dot)K(d)(PAR) and stationary R-rs(555), it was necessary to allow for a declining trend in the ratio of backscattering to total scattering. Within our simulations, this was accomplished by increasing the relative proportion of organic detritus with high mass-specific scattering and low backscattering ratio. An alternative explanation not explicitly modeled is an increasing tendency for the particulate matter to occur in large aggregates. Data to discriminate between these alternatives are not available.
C1 [Gallegos, Charles L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
   [Werdell, P. Jeremy; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Ocean Ecol Branch, Greenbelt, MD 20771 USA.
RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM gallegosc@si.edu
RI Werdell, Jeremy/D-8265-2012; 
OI Gallegos, Charles/0000-0001-5112-0166
NR 75
TC 20
Z9 20
U1 0
U2 14
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 OCT 27
PY 2011
VL 116
AR C00H08
DI 10.1029/2011JC007160
PG 19
WC Oceanography
SC Oceanography
GA 838YH
UT WOS:000296329800003
ER

PT J
AU Manney, GL
   Santee, ML
   Rex, M
   Livesey, NJ
   Pitts, MC
   Veefkind, P
   Nash, ER
   Wohltmann, I
   Lehmann, R
   Froidevaux, L
   Poole, LR
   Schoeberl, MR
   Haffner, DP
   Davies, J
   Dorokhov, V
   Gernandt, H
   Johnson, B
   Kivi, R
   Kyro, E
   Larsen, N
   Levelt, PF
   Makshtas, A
   McElroy, CT
   Nakajima, H
   Parrondo, MC
   Tarasick, DW
   von der Gathen, P
   Walker, KA
   Zinoviev, NS
AF Manney, Gloria L.
   Santee, Michelle L.
   Rex, Markus
   Livesey, Nathaniel J.
   Pitts, Michael C.
   Veefkind, Pepijn
   Nash, Eric R.
   Wohltmann, Ingo
   Lehmann, Ralph
   Froidevaux, Lucien
   Poole, Lamont R.
   Schoeberl, Mark R.
   Haffner, David P.
   Davies, Jonathan
   Dorokhov, Valery
   Gernandt, Hartwig
   Johnson, Bryan
   Kivi, Rigel
   Kyro, Esko
   Larsen, Niels
   Levelt, Pieternel F.
   Makshtas, Alexander
   McElroy, C. Thomas
   Nakajima, Hideaki
   Concepcion Parrondo, Maria
   Tarasick, David W.
   von der Gathen, Peter
   Walker, Kaley A.
   Zinoviev, Nikita S.
TI Unprecedented Arctic ozone loss in 2011
SO NATURE
LA English
DT Article
ID STRATOSPHERIC POLAR VORTEX; MICROWAVE LIMB SOUNDER; NORTHERN-HEMISPHERE;
   CHEMICAL DEPLETION; CLOUD OBSERVATIONS; WINTER 1999/2000; TRANSPORT;
   MLS; CLIMATOLOGY; ANTARCTICA
AB Chemical ozone destruction occurs over both polar regions in local winter-spring. In the Antarctic, essentially complete removal of lower-stratospheric ozone currently results in an ozone hole every year, whereas in the Arctic, ozone loss is highly variable and has until now been much more limited. Here we demonstrate that chemical ozone destruction over the Arctic in early 2011 was-for the first time in the observational record-comparable to that in the Antarctic ozone hole. Unusually long-lasting cold conditions in the Arctic lower stratosphere led to persistent enhancement in ozone-destroying forms of chlorine and to unprecedented ozone loss, which exceeded 80 per cent over 18-20 kilometres altitude. Our results show that Arctic ozone holes are possible even with temperatures much milder than those in the Antarctic. We cannot at present predict when such severe Arctic ozone depletion may be matched or exceeded.
C1 [Manney, Gloria L.; Santee, Michelle L.; Livesey, Nathaniel J.; Froidevaux, Lucien] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
   [Rex, Markus; Wohltmann, Ingo; Lehmann, Ralph; Gernandt, Hartwig; von der Gathen, Peter] Alfred Wegener Inst Polar & Marine Res, D-14473 Potsdam, Germany.
   [Pitts, Michael C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Veefkind, Pepijn; Levelt, Pieternel F.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
   [Veefkind, Pepijn; Levelt, Pieternel F.] Delft Univ Technol, NL-2600 GA Delft, Netherlands.
   [Nash, Eric R.; Haffner, David P.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
   [Poole, Lamont R.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
   [Schoeberl, Mark R.] Sci & Technol Corp, Lanham, MD 20706 USA.
   [Davies, Jonathan; McElroy, C. Thomas; Tarasick, David W.] Environm Canada, Toronto, ON M3H 5T4, Canada.
   [Dorokhov, Valery] Cent Aerol Observ, Dolgoprudnyi 141700, Russia.
   [Johnson, Bryan] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
   [Kivi, Rigel; Kyro, Esko] Finnish Meteorol Inst, Arctic Res Ctr, Sodankyla 99600, Finland.
   [Larsen, Niels] Danish Meteorol Inst, Danish Climate Ctr, DK-2100 Copenhagen, Denmark.
   [Levelt, Pieternel F.] Eindhoven Univ Technol, NL-5600 MB Eindhoven, Netherlands.
   [Makshtas, Alexander; Zinoviev, Nikita S.] Arctic & Antarctic Res Inst, St Petersburg 199397, Russia.
   [Nakajima, Hideaki] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
   [Concepcion Parrondo, Maria] Natl Inst Aerosp Technol, Torrejon De Ardoz 28850, Spain.
   [Walker, Kaley A.] Univ Toronto, Toronto, ON M5S 1A7, Canada.
RP Manney, GL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Gloria.L.Manney@jpl.nasa.gov; Michelle.L.Santee@jpl.nasa.gov
RI von der Gathen, Peter/B-8515-2009; Wohltmann, Ingo/C-1301-2010; Rex,
   Markus/A-6054-2009; Larsen, Niels/G-3145-2014; 
OI von der Gathen, Peter/0000-0001-7409-1556; Wohltmann,
   Ingo/0000-0003-4606-6788; Rex, Markus/0000-0001-7847-8221; Tarasick,
   David/0000-0001-9869-0692
FU OMI; CALIPSO; Match science teams; Aura project; Environment Canada;
   Canadian Space Agency; Academy of Finland; EC DG Research; NASA
FX We thank the MLS (especially A. Lambert, D. Miller, W. Read, M.
   Schwartz, P. Stek, J. Waters), OMI (especially P. K. Bhartia, G. Jaross,
   G. Labow), CALIPSO and Match science teams, as well as A. Douglass, J.
   Joiner and the Aura project, for their support. We also thank W. Daffer
   and R. Fuller for programming assistance at JPL; the many observers
   whose work went into obtaining the ozone-sonde measurements; the ozone
   scientists who participated in the discussion of the 2011 Arctic ozone
   loss and appropriate definition of an Arctic ozone hole (including, but
   not limited to, N. Harris, G. Bodeker, G. Braathen, M. Kurylo, R.
   Salawitch); and especially P. Newman and K. Minschwaner for discussions
   and comments. Meteorological analyses were provided by NASA's Global
   Modeling and Assimilation Office (GMAO) and by the European Centre for
   Medium-Range Weather Forecasts. We thank S. Pawson of GMAO for advice on
   usage of the MERRA reanalysis. Ozone-sonde measurements at Alert,
   Eureka, Resolute Bay, Churchill and Goose Bay were funded by Environment
   Canada. Additional ozone sondes were flown at Eureka as part of the
   Canadian Arctic Atmospheric Chemistry Experiment (ACE) Validation
   Campaign and were funded by the Canadian Space Agency. Academy of
   Finland provided partial funding for performing and processing
   ozone-sonde measurements in Jokioinen and Sodankyla. Ozone soundings and
   work at AWI were partially funded by the EC DG Research through the
   RECONCILE project. Work at the Jet Propulsion Laboratory, California
   Institute of Technology, and at Science Systems and Applications Inc.,
   was done under contract with NASA.
NR 59
TC 238
Z9 255
U1 12
U2 138
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD OCT 27
PY 2011
VL 478
IS 7370
BP 469
EP U65
DI 10.1038/nature10556
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 837JI
UT WOS:000296194200034
PM 21964337
ER

PT J
AU Balcerak, E
   Sullivan, K
AF Balcerak, Ernie
   Sullivan, Kathryn
TI From Space Down to Earth: An Interview With Kathryn Sullivan
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Editorial Material
C1 [Sullivan, Kathryn] Ctr Sci & Ind COSI, Columbus, OH USA.
   [Sullivan, Kathryn] Ohio State Univ, John Glenn Sch Publ Affairs, Battelle Ctr Math & Sci Educ Policy, Columbus, OH 43210 USA.
   [Sullivan, Kathryn] NASA, Washington, DC USA.
EM ebalcerak@agu.org
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD OCT 26
PY 2011
VL 9
AR S10009
DI 10.1029/2011SW000742
PG 3
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
GA 839BE
UT WOS:000296338600002
ER

PT J
AU Kelley, OA
   Halverson, JB
AF Kelley, Owen A.
   Halverson, Jeffrey B.
TI How much tropical cyclone intensification can result from the energy
   released inside of a convective burst?
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID HIGH-RESOLUTION SIMULATION; HURRICANE BONNIE 1998; INNER-CORE;
   PRECIPITATION RADAR; KINEMATIC STRUCTURE; RAPID INTENSIFICATION; LEVEL
   PRESSURE; WATER-BUDGET; SEA SPRAY; PART I
AB This study proposes a framework for estimating how much tropical cyclone intensification could result from the amount of energy released inside of a convective burst. A convective burst is a sequence of vigorous convective cells occupying one portion of a tropical cyclone's eyewall for approximately 9 to 24 h. On the basis of Tropical Rainfall Measuring Mission (TRMM) satellite radar observations and previous modeling studies, a typical convective burst may release in 12 h an extra 6 x 10(17) J of latent heat. TRMM observations suggest that this extra energy represents an increase of 25% or more in the rate that the eyewall releases latent heat prior to the convective burst. Previous studies suggest that 4.5% to 11% of this extra latent heat may be transformed, after a lag of several hours, into an increase in the kinetic energy of the tropical cyclone's inner-core tangential wind. On the basis of the H*wind analysis of aircraft and dropsonde observations, an increase in kinetic energy of this magnitude may be associated with an intensification of 9-16 m s(-1) (17-31 kt) in a tropical cyclone's maximum surface wind. This conservative estimate takes into account the increase in ocean surface friction during the period of intensification and assumes that the associated increase in ocean surface enthalpy flux does not counteract any of the frictional loss. Despite sources of uncertainty, it still appears that significant intensification is possible from the amount of energy released inside of a typical convective burst.
C1 [Kelley, Owen A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Kelley, Owen A.] George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
   [Halverson, Jeffrey B.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
RP Kelley, OA (reprint author), NASA, Goddard Space Flight Ctr, Code 610-2,Bldg 32,Rm S048B, Greenbelt, MD 20771 USA.
EM owen.kelley@nasa.gov
FU NASA [NNX07AJ22A, NNH08ZDA001N-HRSP]
FX TRMM satellite data was provided by NASA and JAXA. H*wind analysis
   provided by NOAA's Hurricane Research Division. The first author would
   like to thank his Ph.D. advisor, Michael Summers, for providing feedback
   on early results related to this study. The first author was supported
   through NASA grant NNX07AJ22A. The second author was supported in part
   by NASA grant NNH08ZDA001N-HRSP. Both authors would like to thank Ramesh
   Kakar for his continued support of TRMM. Three anonymous reviewers
   provided suggestions that significantly strengthened this text.
   Computational facilities were provided by the Precipitation Processing
   System at NASA Goddard.
NR 69
TC 4
Z9 4
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 25
PY 2011
VL 116
AR D20118
DI 10.1029/2011JD015954
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 839AI
UT WOS:000296336300002
ER

PT J
AU Bueno, J
   Llombart, N
   Day, PK
   Echternach, PM
AF Bueno, J.
   Llombart, N.
   Day, P. K.
   Echternach, P. M.
TI Optical characterization of the quantum capacitance detector at 200 mu m
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID SPICA; ASTRONOMY; TES
AB We present the optical characterization at 200 mu m wavelength of an antenna coupled quantum capacitance detector (QCD), a cryogenic detector based on a single Cooper pair box (SCB). The response of the device to a cryogenic blackbody source and the device noise have been measured giving an optical noise-equivalent power (NEP) at a readout frequency of 10 kHz of 2 x 10(-17) W/Hz(1/2) at an optical loading of 17 fW. For optical loadings of a few pW, the optical NEP was on the order of 10(-16) W/Hz(1/2), demonstrating that QCDs could already work as detectors for far-infrared and submillimeter wave radiation in a ground based telescope. (C) 2011 American Institute of Physics. [doi:10.1063/1.3651277]
C1 [Bueno, J.; Llombart, N.; Day, P. K.; Echternach, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bueno, J (reprint author), Ctr Astrobiol CSIC INTA, 28850 Torrejon Ardoz, Madrid, Spain.
EM juan.bueno@cab.inta-csic.es
FU National Aeronautics and Space Administration; Ramon y Cajal
   [RYC200904924];  [AYA 2008 - 06166C0302];  [AYA201021697C0501];  [AYA
   201010054E]
FX We would like to thank Ken Cooper, Boris Karasik, Per Delsing, and Jonas
   Zmuidzinas for helpful discussions, Jon Kawamura for helping with the
   optical system, and Richard Muller for performing electron-beam
   lithography. This work was performed at the Jet Propulsion Laboratory,
   California Institute of Technology, under a contract with the National
   Aeronautics and Space Administration. Juan Bueno acknowledges support
   through Grant Nos. AYA 2008 - 06166C0302 and AYA201021697C0501. Nuria
   Llombart acknowledges support through Grant No. AYA 201010054E and the
   program "Ramon y Cajal" RYC200904924.
NR 20
TC 2
Z9 2
U1 3
U2 5
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
   MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD OCT 24
PY 2011
VL 99
IS 17
AR 173503
DI 10.1063/1.3651277
PG 3
WC Physics, Applied
SC Physics
GA 841NG
UT WOS:000296518400068
ER

PT J
AU Silvestro, S
   Vaz, DA
   Fenton, LK
   Geissler, PE
AF Silvestro, S.
   Vaz, D. A.
   Fenton, L. K.
   Geissler, P. E.
TI Active aeolian processes on Mars: A regional study in Arabia and
   Meridiani Terrae
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ORBITER CAMERA; SEDIMENT; DUNES
AB We present evidence of widespread aeolian activity in the Arabia Terra/Meridiani region (Mars), where different kinds of aeolian modifications have been detected and classified. Passing from the regional to the local scale, we describe one particular dune field in Meridiani Planum, where two ripple populations are distinguished by means of different migration rates. Moreover, a consistent change in the ripple pattern is accompanied by significant dune advancement (between 0.4-1 meter in one Martian year) that is locally triggered by large avalanche features. This suggests that dune advancement may be common throughout the Martian tropics. Citation: Silvestro, S., D. A. Vaz, L. K. Fenton, and P. E. Geissler (2011), Active aeolian processes on Mars: A regional study in Arabia and Meridiani Terrae, Geophys. Res. Lett., 38, L20201, doi: 10.1029/2011GL048955.
C1 [Silvestro, S.; Fenton, L. K.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
   [Vaz, D. A.] Univ Coimbra, Ctr Geophys, P-3000134 Coimbra, Portugal.
   [Fenton, L. K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Geissler, P. E.] US Geol Survey, Flagstaff, AZ 86001 USA.
RP Silvestro, S (reprint author), SETI Inst, Carl Sagan Ctr, 189 N Bernardo Ave,Ste 100, Mountain View, CA 94043 USA.
EM ssilvestro@seti.org
RI Vaz, David/M-4702-2013
OI Vaz, David/0000-0002-3583-2267
FU NASA [NNH09ZDA001N]; FCT (Fundacao para a Ciencia e a Tecnologia)
   [SFRH/BPD/72371/2010]
FX This research was supported by a grant from the NASA Mars Data Analysis
   program (NNH09ZDA001N). We acknowledge Nathan Bridges for providing
   unreleased HiRISE images in Trouvelot crater, Bob Craddock and an
   anonymous reviewer for their helpful comments and suggestions. D. Vaz
   acknowledges the support given by FCT (Fundacao para a Ciencia e a
   Tecnologia - SFRH/BPD/72371/2010). English editing by Noah Hammond is
   also gratefully acknowledged.
NR 22
TC 24
Z9 24
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 22
PY 2011
VL 38
AR L20201
DI 10.1029/2011GL048955
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 836YY
UT WOS:000296157300002
ER

PT J
AU Li, J
   Carlson, BE
   Lacis, AA
AF Li, Jing
   Carlson, Barbara E.
   Lacis, Andrew A.
TI El Nino-Southern Oscillation correlated aerosol Angstrom exponent
   anomaly over the tropical Pacific discovered in satellite measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID INTERANNUAL VARIABILITY; IMAGING SPECTRORADIOMETER; TROPOSPHERIC OZONE;
   OPTICAL-THICKNESS; CLIMATE-CHANGE; FOREST-FIRE; MODIS; OCEAN; PRODUCTS;
   LAND
AB El Nino-Southern Oscillation (ENSO) is the dominant mode of interannual variability in the tropical atmosphere. ENSO could potentially impact local and global aerosol properties through atmospheric circulation anomalies and teleconnections. By analyzing aerosol properties, including aerosol optical depth (AOD) and Angstrom exponent (AE; often used as a qualitative indicator of aerosol particle size) from the Moderate Resolution Imaging Spectrometer, the Multiangle Imaging Spectroradiometer and the Sea-viewing Wide Field-of-view Sensor for the period 2000-2011, we find a strong correlation between the AE data and the multivariate ENSO index (MEI) over the tropical Pacific. Over the western tropical Pacific (WTP), AE increases during El Nino events and decreases during La Nina events, while the opposite is true over the eastern tropical Pacific (ETP). The difference between AE anomalies in the WTP and ETP has a higher correlation coefficient (>0.7) with the MEI than the individual time series and could be considered another type of ENSO index. As no significant ENSO correlation is found in AOD over the same region, the change in AE (and hence aerosol size) is likely to be associated with aerosol composition changes due to anomalous meteorological conditions induced by the ENSO. Several physical parameters or mechanisms that might be responsible for the correlation are discussed. Preliminary analysis indicates surface wind anomaly might be the major contributor, as it reduces sea-salt production and aerosol transport during El Nino events. Precipitation and cloud fraction are also found to be correlated with tropical Pacific AE. Possible mechanisms, including wet removal and cloud shielding effects, are considered. Variations in relative humidity, tropospheric ozone concentration, and ocean color during El Nino have been ruled out. Further investigation is needed to fully understand this AE-ENSO covariability and the underlying physical processes responsible for it.
C1 [Li, Jing; Carlson, Barbara E.] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA.
   [Li, Jing; Lacis, Andrew A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Li, J (reprint author), Columbia Univ, Dept Earth & Environm Sci, 2960 Broadway, New York, NY 10027 USA.
EM jli@giss.nasa.gov
RI Carlson, Barbara/D-8319-2012; Li, Jing/J-2397-2014
OI Li, Jing/0000-0002-0540-0412
NR 43
TC 8
Z9 8
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 OCT 22
PY 2011
VL 116
AR D20204
DI 10.1029/2011JD015733
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 837AB
UT WOS:000296161400001
ER

PT J
AU McKee, M
   Squyres, S
AF McKee, Maggie
   Squyres, Steven
TI One minute with ... Steven Squyres
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [Squyres, Steven] Cornell Univ, Ithaca, NY USA.
   [Squyres, Steven] NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD OCT 22
PY 2011
VL 212
IS 2835
BP 31
EP 31
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 838PA
UT WOS:000296303500016
ER

PT J
AU Amendola, G
   Arnieri, E
   Boccia, L
   Borgia, A
   Focardi, P
   Russo, I
AF Amendola, G.
   Arnieri, E.
   Boccia, L.
   Borgia, A.
   Focardi, P.
   Russo, I.
TI Hybrid waveguide-stripline feeding network for dual polarised arrays at
   K band
SO IET MICROWAVES ANTENNAS & PROPAGATION
LA English
DT Article
ID ANTENNA-ARRAY; MICROSTRIP ARRAY; HIGH-EFFICIENCY
AB This study demonstrates a hybrid technology for the implementation of efficient feeding networks in K-band arrays. In the proposed hybrid structure, the main part of the distribution network consists of dielectric-loaded E-plane metallic waveguides, whereas stripline circuits that depart from the waveguides are used to feed the radiators. The efficiency of the hybrid feeding network is verified on a 4 x 4 dual-polarised array of circular waveguides operating in the K band. Details on the characteristics of the loaded waveguide and the array elements, and on the construction of the overall structure are given. Measured results are presented and discussed in order to demonstrate that the hybrid waveguide-stripline structures are a promising technology for the creation of efficient feeding networks at higher frequencies.
C1 [Amendola, G.; Arnieri, E.; Boccia, L.; Borgia, A.; Russo, I.] Univ Calabria, Dept Elettron Comp Sci & Syst, I-87036 Arcavacata Di Rende, CS, Italy.
   [Focardi, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Amendola, G (reprint author), Univ Calabria, Dept Elettron Comp Sci & Syst, Via P Bucci, I-87036 Arcavacata Di Rende, CS, Italy.
EM earnieri@deis.unical.it
OI Borgia, Antonio/0000-0001-5418-3779; arnieri, emilio/0000-0003-2089-9757
FU National Aeronautics and Space Administration
FX The authors wish to thank Alfredo Catalani of Space Engineering (Rome,
   Italy) for performing the measurements on the array prototype. The
   research described in this paper was partly carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration.
NR 19
TC 10
Z9 10
U1 0
U2 2
PU INST ENGINEERING TECHNOLOGY-IET
PI HERTFORD
PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND
SN 1751-8725
J9 IET MICROW ANTENNA P
JI IET Microw. Antennas Propag.
PD OCT 21
PY 2011
VL 5
IS 13
BP 1568
EP 1575
DI 10.1049/iet-map.2011.0018
PG 8
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 851JY
UT WOS:000297266100006
ER

PT J
AU Hong, J
   Allen, B
   Grindlay, J
   Barthelemy, S
   Baker, R
   Garson, A
   Krawczynski, H
   Apple, J
   Cleveland, WH
AF Hong, J.
   Allen, B.
   Grindlay, J.
   Barthelemy, S.
   Baker, R.
   Garson, A.
   Krawczynski, H.
   Apple, J.
   Cleveland, W. H.
TI Flight performance of an advanced CZT imaging detector in a
   balloon-borne wide-field hard X-ray telescope-ProtoEXIST1
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
   SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Hard X-ray imaging; CdZnTe; Coded-aperture imaging
AB We successfully carried out the first high-altitude balloon flight of a wide-field hard X-ray coded-aperture telescope ProtoEXIST1, which was launched from the Columbia Scientific Balloon Facility at Ft. Sumner, New Mexico on October 9, 2009. ProtoEXIST1 is the first implementation of an advanced CdZnTe (CZT) imaging detector in our ongoing program to establish the technology required for next generation wide-field hard X-ray telescopes such as the High Energy Telescope (HET) in the Energetic X-ray Imaging Survey Telescope (EXIST). The CZT detector plane in ProtoEXIST1 consists of an 8 x 8 array of closely tiled 2 cm x 2 cm x 0.5 cm thick pixellated CZT crystals, each with 8 x 8 pixels, mounted on a set of readout electronics boards and covering a 256 cm(2) active area with 2.5 mm pixels. A tungsten mask, mounted at 90 cm above the detector provides shadowgrams of X-ray sources in the 30-600 keV band for imaging, allowing a fully coded field of view of 9 degrees x 9 degrees (and 19 degrees x 19 degrees for 50% coding fraction) with an angular resolution of 20'. In order to reduce the background radiation, the detector is surrounded by semi-graded (Pb/Sn/Cu) passive shields on the four sides all the way to the mask. On the back side, a 26 cm x 26 cm x 2 cm CsI(Na) active shield provides signals to tag charged particle induced events as well as greater than or similar to 100 keV background photons from below. The flight duration was only about 7.5 h due to strong winds (60 knots) at float altitude (38-39 km). Throughout the flight, the CZT detector performed excellently. The telescope observed Cyg X-1, a bright black hole binary system, for similar to 1 h at the end of the flight. Despite a few problems with the pointing and aspect systems that caused the telescope to track about 6.4 degrees off the target, the analysis of the Cyg X-1 data revealed an X-ray source at 7.2 sigma in the 30-100 key energy band at the expected location from the optical images taken by the onboard daytime star camera. The success of this first flight is very encouraging for the future development of the advanced CZT imaging detectors (ProtoEXIST2, with 0.6 mm pixels), which will take advantage of the modularization architecture employed in ProtoEXIST1. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Hong, J.; Allen, B.; Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Barthelemy, S.; Baker, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Garson, A.; Krawczynski, H.] Washington Univ, St Louis, MO 63130 USA.
   [Garson, A.; Krawczynski, H.] McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
   [Apple, J.; Cleveland, W. H.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Apple, J.; Cleveland, W. H.] Univ Space Res Assoc, Huntsville, AL 35812 USA.
RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jaesub@head.cfa.harvard.edu
FU NASA [NNG06WC12G, NNXO9AD76G, NNX10AJ56G]
FX This work was supported by NASA Grants NNG06WC12G and NNXO9AD76G to
   Harvard University, and NASA Grant NNX10AJ56G to Washington University
   in St. Louis. We thank M. Burke (SAO engineering), N. Gehrels (GSFC), K.
   Dietz, C.M. Benson, B. Ramsey (MSFC), D. Huie (University of Alabama
   Hunsville), W.R. Cook and F. Harrison (Caltech) for their support in the
   development and assembly of the ProtoEXIST1 detector, telescope and
   gondola. We also thank the McDonnell Center for the Space Sciences for
   their support in the active CsI shield assembly, and the NASA CSBF
   balloon launching team for their excellent support.
NR 18
TC 6
Z9 6
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
   Equip.
PD OCT 21
PY 2011
VL 654
IS 1
BP 361
EP 372
DI 10.1016/j.nima.2011.07.025
PG 12
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
   Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 831XT
UT WOS:000295765100051
ER

PT J
AU Lubelsmeyer, K
   von Dratzig, AS
   Wlochal, M
   Ambrosi, G
   Azzarello, P
   Battiston, R
   Becker, R
   Becker, U
   Bertucci, B
   Bollweg, K
   Burger, JD
   Cadoux, F
   Cai, XD
   Capell, M
   Choutko, V
   Duranti, M
   Gargiulo, C
   Guandalini, C
   Haino, S
   Ionica, M
   Koulemzine, A
   Kounine, A
   Koutsenko, V
   Laurenti, G
   Lebedev, A
   Martin, T
   Oliva, A
   Paniccia, M
   Perrin, E
   Rapin, D
   Rozhkov, A
   Schael, S
   Tholen, H
   Ting, SCC
   Zuccon, P
AF Luebelsmeyer, K.
   von Dratzig, A. Schultz
   Wlochal, M.
   Ambrosi, G.
   Azzarello, P.
   Battiston, R.
   Becker, R.
   Becker, U.
   Bertucci, B.
   Bollweg, K.
   Burger, J. D.
   Cadoux, F.
   Cai, X. D.
   Capell, M.
   Choutko, V.
   Duranti, M.
   Gargiulo, C.
   Guandalini, C.
   Haino, S.
   Ionica, M.
   Koulemzine, A.
   Kounine, A.
   Koutsenko, V.
   Laurenti, G.
   Lebedev, A.
   Martin, T.
   Oliva, A.
   Paniccia, M.
   Perrin, E.
   Rapin, D.
   Rozhkov, A.
   Schael, St
   Tholen, H.
   Ting, S. C. C.
   Zuccon, P.
TI Upgrade of the Alpha Magnetic Spectrometer (AMS-02) for long term
   operation on the International Space Station (ISS)
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
   SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Astro_particle physics; AMS-02
AB Following the decision to maintain the International Space Station (ISS) on orbit until at least 2020 (possibly until 2028) the AMS collaboration decided to correspondingly extend the lifetime of the experiment. Since the limited amount of helium used to cool the superconducting magnet allowed for only a limited run time of the experiment, a change from the superconducting magnet to the permanent magnet used in AMS-01 became necessary. Due to the lower magnetic field, to maintain the resolution the silicon tracker also had to be reconfigured with the installation of a silicon plane on the top of the experiment and a new plane above the electromagnetic calorimeter. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Luebelsmeyer, K.; von Dratzig, A. Schultz; Wlochal, M.; Schael, St; Tholen, H.] Rhein Westfal TH Aachen, Inst Phys 1, D-52074 Aachen, Germany.
   [Cadoux, F.; Paniccia, M.; Perrin, E.; Rapin, D.] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland.
   [Guandalini, C.; Laurenti, G.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
   [Ambrosi, G.; Azzarello, P.; Battiston, R.; Bertucci, B.; Duranti, M.; Haino, S.; Ionica, M.; Oliva, A.; Zuccon, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06100 Perugia, Italy.
   [Battiston, R.; Bertucci, B.; Duranti, M.; Ionica, M.] Univ Perugia, I-06100 Perugia, Italy.
   [Gargiulo, C.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
   [Becker, R.; Becker, U.; Burger, J. D.; Cai, X. D.; Capell, M.; Choutko, V.; Koulemzine, A.; Kounine, A.; Koutsenko, V.; Lebedev, A.; Rozhkov, A.; Ting, S. C. C.] MIT, Cambridge, MA 02139 USA.
   [Bollweg, K.; Martin, T.] NASA, JSC Houston, Houston, TX 77058 USA.
RP von Dratzig, AS (reprint author), Rhein Westfal TH Aachen, Inst Phys 1, D-52074 Aachen, Germany.
EM svd@physik.rwth-aachen.de
RI Zuccon, Paolo/I-7736-2012; bertucci, bruna/J-5237-2012; Duranti,
   Matteo/I-7691-2013; Paniccia, Mercedes/A-4519-2017; 
OI Zuccon, Paolo/0000-0002-2728-0167; Duranti, Matteo/0000-0003-0980-6425;
   Paniccia, Mercedes/0000-0001-8482-2703; Ambrosi,
   Giovanni/0000-0001-6977-9559; Bertucci, Bruna/0000-0001-7584-293X
FU INFN, Italy; University of Geneva, Switzerland; RWTH Aachen, Germany; US
   DOE; MIT; NASA; space agencies of Germany (DLR); Italy (ASI)
FX The support of INFN, Italy, the University of Geneva, Switzerland, the
   RWTH Aachen, Germany, the US DOE and MIT and NASA is gratefully
   acknowledged. Support from the space agencies of Germany (DLR) and Italy
   (ASI) played important roles in the success of the reconfiguration of
   AMS-02.
NR 4
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U1 0
U2 24
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
   Equip.
PD OCT 21
PY 2011
VL 654
IS 1
BP 639
EP 648
DI 10.1016/j.nima.2011.06.051
PG 10
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
   Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 831XT
UT WOS:000295765100092
ER

PT J
AU Hogerheijde, MR
   Bergin, EA
   Brinch, C
   Cleeves, LI
   Fogel, JKJ
   Blake, GA
   Dominik, C
   Lis, DC
   Melnick, G
   Neufeld, D
   Panic, O
   Pearson, JC
   Kristensen, L
   Yildiz, UA
   van Dishoeck, EF
AF Hogerheijde, Michiel R.
   Bergin, Edwin A.
   Brinch, Christian
   Cleeves, L. Ilsedore
   Fogel, Jeffrey K. J.
   Blake, Geoffrey A.
   Dominik, Carsten
   Lis, Dariusz C.
   Melnick, Gary
   Neufeld, David
   Panic, Olja
   Pearson, John C.
   Kristensen, Lars
   Yildiz, Umut A.
   van Dishoeck, Ewine F.
TI Detection of the Water Reservoir in a Forming Planetary System
SO SCIENCE
LA English
DT Article
ID T TAURI STARS; PROTOPLANETARY DISKS; HERSCHEL; LINES; ICE; INTERSTELLAR;
   EMISSION; SURFACE; REGION; GRAINS
AB Icy bodies may have delivered the oceans to the early Earth, yet little is known about water in the ice-dominated regions of extrasolar planet-forming disks. The Heterodyne Instrument for the Far-Infrared on board the Herschel Space Observatory has detected emission lines from both spin isomers of cold water vapor from the disk around the young star TW Hydrae. This water vapor likely originates from ice-coated solids near the disk surface, hinting at a water ice reservoir equivalent to several thousand Earth oceans in mass. The water's ortho-to-para ratio falls well below that of solar system comets, suggesting that comets contain heterogeneous ice mixtures collected across the entire solar nebula during the early stages of planetary birth.
C1 [Hogerheijde, Michiel R.; Brinch, Christian; Kristensen, Lars; Yildiz, Umut A.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
   [Bergin, Edwin A.; Cleeves, L. Ilsedore; Fogel, Jeffrey K. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
   [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Dominik, Carsten] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
   [Lis, Dariusz C.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
   [Melnick, Gary] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Neufeld, David] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
   [Panic, Olja] European So Observ, D-85748 Garching, Germany.
   [Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Hogerheijde, MR (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM michiel@strw.leidenuniv.nl
RI Kristensen, Lars/F-4774-2011; Yildiz, Umut/C-5257-2011; Brinch,
   Christian/G-5157-2015
OI Kristensen, Lars/0000-0003-1159-3721; Yildiz, Umut/0000-0001-6197-2864;
   Brinch, Christian/0000-0002-5074-7183
FU Nederlandse Organisatie voor Wetenschappelijk Onderzoek [639.042.404];
   NSF [0707777]; NASA
FX Herschel is a European Space Agency space observatory with science
   instruments provided by European-led principal investigator consortia
   and with important participation from NASA. This work was partially
   supported by Nederlandse Organisatie voor Wetenschappelijk Onderzoek
   grant 639.042.404, NSF grant 0707777, and, as part of the NASA Herschel
   HIFI guaranteed time program, NASA. The data presented here are archived
   at the Herschel Science Archive, http://archives.esac.esa.int/hda/ui,
   under OBSID 1342198337 and 1342201585.
NR 24
TC 106
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U1 4
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PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD OCT 21
PY 2011
VL 334
IS 6054
BP 338
EP 340
DI 10.1126/science.1208931
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 835RC
UT WOS:000296052500042
PM 22021851
ER

PT J
AU Cox, P
   Krips, M
   Neri, R
   Omont, A
   Gusten, R
   Menten, KM
   Wyrowski, F
   Weiss, A
   Beelen, A
   Gurwell, MA
   Dannerbauer, H
   Ivison, RJ
   Negrello, M
   Aretxaga, I
   Hughes, DH
   Auld, R
   Baes, M
   Blundell, R
   Buttiglione, S
   Cava, A
   Cooray, A
   Dariush, A
   Dunne, L
   Dye, S
   Eales, SA
   Frayer, D
   Fritz, J
   Gavazzi, R
   Hopwood, R
   Ibar, E
   Jarvis, M
   Maddox, S
   Michallowski, M
   Pascale, E
   Pohlen, M
   Rigby, E
   Smith, DJB
   Swinbank, AM
   Temi, P
   Valtchanov, I
   van der Werf, P
   de Zotti, G
AF Cox, P.
   Krips, M.
   Neri, R.
   Omont, A.
   Guesten, R.
   Menten, K. M.
   Wyrowski, F.
   Weiss, A.
   Beelen, A.
   Gurwell, M. A.
   Dannerbauer, H.
   Ivison, R. J.
   Negrello, M.
   Aretxaga, I.
   Hughes, D. H.
   Auld, R.
   Baes, M.
   Blundell, R.
   Buttiglione, S.
   Cava, A.
   Cooray, A.
   Dariush, A.
   Dunne, L.
   Dye, S.
   Eales, S. A.
   Frayer, D.
   Fritz, J.
   Gavazzi, R.
   Hopwood, R.
   Ibar, E.
   Jarvis, M.
   Maddox, S.
   Michallowski, M.
   Pascale, E.
   Pohlen, M.
   Rigby, E.
   Smith, D. J. B.
   Swinbank, A. M.
   Temi, P.
   Valtchanov, I.
   van der Werf, P.
   de Zotti, G.
TI GAS AND DUST IN A SUBMILLIMETER GALAXY AT z=4.24 FROM THE HERSCHEL ATLAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: high-redshift;
   galaxies: individual (ID 141); galaxies: starburst; submillimeter:
   galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; ISO-LWS SPECTROSCOPY; MICRON LINE
   DEFICIT; STAR-FORMATION; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; ATOMIC
   CARBON; MU-M; MOLECULAR GAS; PHYSICAL CONDITIONS
AB We report ground-based follow-up observations of the exceptional source, ID 141, one of the brightest sources detected so far in the Herschel Astrophysical Terahertz Large Area Survey cosmological survey. ID 141 was observed using the IRAM 30 m telescope and Plateau de Bure interferometer (PdBI), the Submillimeter Array, and the Atacama Pathfinder Experiment submillimeter telescope to measure the dust continuum and emission lines of the main isotope of carbon monoxide and carbon ([C I] and [C II]). The detection of strong CO emission lines with the PdBI confirms that ID 141 is at high redshift (z = 4.243 +/- 0.001). The strength of the continuum and emission lines suggests that ID 141 is gravitationally lensed. The width (Delta V-FWHM similar to 800 km s(-1)) and asymmetric profiles of the CO and carbon lines indicate orbital motion in a disk or a merger. The properties derived for ID 141 are compatible with an ultraluminous (L-FIR similar to (8.5 +/- 0.3) x 10(13) mu(-1)(L) L-circle dot, where mu L is the amplification factor), dense (n approximate to 10(4) cm(-3)), and warm (T-kin approximate to 40 K) starburst galaxy, with an estimated star formation rate of (0.7-1.7) x 10(4) mu(-1)(L) M-circle dot yr(-1). The carbon emission lines indicate a dense (n approximate to 10(4) cm(-3)) photon-dominated region, illuminated by a far-UV radiation field a few thousand times more intense than that in our Galaxy. In conclusion, the physical properties of the high-z galaxy ID 141 are remarkably similar to those of local ultraluminous infrared galaxies.
C1 [Cox, P.; Krips, M.; Neri, R.] IRAM, F-38406 St Martin Dheres, France.
   [Omont, A.; Gavazzi, R.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
   [Omont, A.; Gavazzi, R.] CNRS, UMR7095, F-75014 Paris, France.
   [Guesten, R.; Menten, K. M.; Wyrowski, F.; Weiss, A.] MPIfR, D-53121 Bonn, Germany.
   [Beelen, A.] Univ Paris 11, IAS, F-91405 Orsay, France.
   [Gurwell, M. A.; Blundell, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Dannerbauer, H.] CEA DSM CNRS Univ Paris Diderot, DAPNIA Serv Astrophys, CEA Saclay, AIM, F-91191 Gif Sur Yvette, France.
   [Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Ivison, R. J.; Michallowski, M.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Negrello, M.; Hopwood, R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
   [Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico.
   [Auld, R.; Dariush, A.; Eales, S. A.; 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.
   [Buttiglione, S.; Jarvis, M.; de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
   [Buttiglione, S.; Jarvis, M.; de Zotti, G.] SISSA, I-34136 Trieste, Italy.
   [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
   [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran.
   [Dunne, L.; Dye, S.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
   [Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
   [Swinbank, A. M.] Univ Durham, Inst Computat Cosmol, Durham DH1 3EE, England.
   [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
   [Valtchanov, I.] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain.
   [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Cox, P (reprint author), IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France.
EM cox@iram.fr
RI Baes, Maarten/I-6985-2013; Ivison, R./G-4450-2011; Cava,
   Antonio/C-5274-2017; 
OI Baes, Maarten/0000-0002-3930-2757; Ivison, R./0000-0001-5118-1313; Cava,
   Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X; Dye,
   Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X
FU NASA through JPL; Centre National de la Recherche Scientifique (France);
   Max-Planck Gesellschaft (Germany); Instituto Geografico Nacional
   (Spain); Smithsonian Institution; Academia Sinica; CONACyT [39953-F]; 
   [ASI-INAF I009/10/0]
FX The results described in this paper are based on observations obtained
   with Herschel, an ESA space observatory with science instruments
   provided by European-led Principal Investigator consortia and with
   important participation from NASA. US participants in H-ATLAS
   acknowledge support from NASA through a contract from JPL. The
   ground-based follow-up observations were obtained at the following
   facilities. The 30 m telescope and the PdBI of IRAM that is funded by
   the Centre National de la Recherche Scientifique (France), the
   Max-Planck Gesellschaft (Germany), and the Instituto Geografico Nacional
   (Spain). APEX is a collaboration between the Max-Planck-Institut fur
   Radioastronomie, the European Southern Observatory, and the Onsala Space
   Observatory. The Submillimeter Array (SMA) is a joint project between
   the Smithsonian Astrophysical Observatory and the Academia Sinica
   Institute of Astronomy and Astrophysics and is funded by the Smithsonian
   Institution and the Academia Sinica. Part of this study was supported by
   financial contribution from the agreement ASI-INAF I009/10/0 and by
   CONACyT grant 39953-F.
NR 69
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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 OCT 20
PY 2011
VL 740
IS 2
AR 63
DI 10.1088/0004-637X/740/2/63
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900013
ER

PT J
AU Gogus, E
   Woods, PM
   Kouveliotou, C
   Finger, MH
   Pal'shin, V
   Kaneko, Y
   Golenetskii, S
   Frederiks, D
   Airhart, C
AF Gogus, Ersin
   Woods, Peter M.
   Kouveliotou, Chryssa
   Finger, Mark H.
   Pal'shin, Valentin
   Kaneko, Yuki
   Golenetskii, Sergey
   Frederiks, Dmitry
   Airhart, Carol
TI EXTENDED TAILS FROM SGR 1806-20 BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (SGR 1806-20); X-rays: bursts
ID X-RAY OSCILLATIONS; GAMMA-REPEATER SGR-1900+14; GIANT FLARE; STATISTICAL
   PROPERTIES; SGR-1806-20; EMISSION; HYPERFLARE; ACTIVATION; DISCOVERY;
   PULSARS
AB In 2004, SGR 1806-20 underwent a period of intense and long-lasting burst activity that included the giant flare of 2004 December 27-the most intense extra-solar transient event ever detected at Earth. During this active episode, we routinely monitored the source with Rossi X-ray Timing Explorer and occasionally with Chandra. During the course of these observations, we identified two relatively bright bursts observed with Konus-Wind in hard X-rays that were followed by extended X-ray tails or afterglows lasting hundreds to thousands of seconds. Here, we present detailed spectral and temporal analysis of these events observed about 6 and 1.5 months prior to the 2004 December 27 giant flare. We find that both X-ray tails are consistent with a cooling blackbody of constant radius. These spectral results are qualitatively similar to those of the burst afterglows recorded from SGR 1900+14 and recently from SGR 1550-5418. However, the latter two sources exhibit significant increase in their pulsed X-ray intensity following the burst, while we did not detect any significant changes in the rms pulsed amplitude during the SGR 1806-20 events. Moreover, we find that the fraction of energy partitioned to the burst (prompt energy release) and the tail (afterglow) differs by an order of magnitude between SGR 1900+14 and SGR 1806-20. We suggest that such differences can be attributed to differences in the crustal heating mechanism of these neutron stars combined with the geometry of the emitting areas.
C1 [Gogus, Ersin; Kaneko, Yuki] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
   [Woods, Peter M.] Corvid Technol, Huntsville, AL 35806 USA.
   [Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP 62, Huntsville, AL 35812 USA.
   [Finger, Mark H.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
   [Pal'shin, Valentin; Golenetskii, Sergey; Frederiks, Dmitry] Russian Acad Sci, AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
   [Pal'shin, Valentin] St Petersburg State Polytech Univ, St Petersburg 195251, Russia.
   [Airhart, Carol] Dynetics Inc, Huntsville, AL 35806 USA.
RP Gogus, E (reprint author), Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
EM ersing@sabanciuniv.edu
RI Frederiks, Dmitry/C-7612-2014; Pal'shin, Valentin/F-3973-2014;
   Golenetskii, Sergey/B-3818-2015; 
OI Frederiks, Dmitry/0000-0002-1153-6340
FU Scientific and Technological Council of Turkey (TUBITAK) [109T755];
   Russian Space Agency; RFBR [09-02-00166a]; Ministry of Education and
   Science of Russian Federation [11.G34.31.0001]
FX E.G. and Y.K. acknowledge the support from the Scientific and
   Technological Council of Turkey (TUBITAK) through grant 109T755. The
   Konus-Wind experiment is supported by a Russian Space Agency contract
   and RFBR grant 09-02-00166a. V.P. acknowledges support from the Ministry
   of Education and Science of Russian Federation (contract 11.G34.31.0001
   with SPbSPU and Leading Scientist G. G. Pavlov).
NR 32
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
IS 2
AR 55
DI 10.1088/0004-637X/740/2/55
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900005
ER

PT J
AU Hajian, A
   Acquaviva, V
   Ade, PAR
   Aguirre, P
   Amiri, M
   Appel, JW
   Barrientos, LF
   Battistelli, ES
   Bond, JR
   Brown, B
   Burger, B
   Chervenak, J
   Das, S
   Devlin, MJ
   Dicker, SR
   Doriese, WB
   Dunkley, J
   Dunner, R
   Essinger-Hileman, T
   Fisher, RP
   Fowler, JW
   Halpern, M
   Hasselfield, M
   Hernandez-Monteagudo, C
   Hilton, GC
   Hilton, M
   Hincks, AD
   Hlozek, R
   Huffenberger, KM
   Hughes, DH
   Hughes, JP
   Infante, L
   Irwin, KD
   Juin, JB
   Kaul, M
   Klein, J
   Kosowsky, A
   Lau, JM
   Limon, M
   Lin, YT
   Lupton, RH
   Marriage, TA
   Marsden, D
   Mauskopf, P
   Menanteau, F
   Moodley, K
   Moseley, H
   Netterfield, CB
   Niemack, MD
   Nolta, MR
   Page, LA
   Parker, L
   Partridge, B
   Reid, B
   Sehgal, N
   Sherwin, BD
   Sievers, J
   Spergel, DN
   Staggs, ST
   Swetz, DS
   Switzer, ER
   Thornton, R
   Trac, H
   Tucker, C
   Warne, R
   Wollack, E
   Zhao, Y
AF Hajian, Amir
   Acquaviva, Viviana
   Ade, Peter A. R.
   Aguirre, Paula
   Amiri, Mandana
   Appel, John William
   Felipe Barrientos, L.
   Battistelli, Elia S.
   Bond, John R.
   Brown, Ben
   Burger, Bryce
   Chervenak, Jay
   Das, Sudeep
   Devlin, Mark J.
   Dicker, Simon R.
   Doriese, W. Bertrand
   Dunkley, Joanna
   Duenner, Rolando
   Essinger-Hileman, Thomas
   Fisher, Ryan P.
   Fowler, Joseph W.
   Halpern, Mark
   Hasselfield, Matthew
   Hernandez-Monteagudo, Carlos
   Hilton, Gene C.
   Hilton, Matt
   Hincks, Adam D.
   Hlozek, Renee
   Huffenberger, Kevin M.
   Hughes, David H.
   Hughes, John P.
   Infante, Leopoldo
   Irwin, Kent D.
   Baptiste Juin, Jean
   Kaul, Madhuri
   Klein, Jeff
   Kosowsky, Arthur
   Lau, Judy M.
   Limon, Michele
   Lin, Yen-Ting
   Lupton, Robert H.
   Marriage, Tobias A.
   Marsden, Danica
   Mauskopf, Phil
   Menanteau, Felipe
   Moodley, Kavilan
   Moseley, Harvey
   Netterfield, Calvin B.
   Niemack, Michael D.
   Nolta, Michael R.
   Page, Lyman A.
   Parker, Lucas
   Partridge, Bruce
   Reid, Beth
   Sehgal, Neelima
   Sherwin, Blake D.
   Sievers, Jon
   Spergel, David N.
   Staggs, Suzanne T.
   Swetz, Daniel S.
   Switzer, Eric R.
   Thornton, Robert
   Trac, Hy
   Tucker, Carole
   Warne, Ryan
   Wollack, Ed
   Zhao, Yue
TI THE ATACAMA COSMOLOGY TELESCOPE: CALIBRATION WITH THE WILKINSON
   MICROWAVE ANISOTROPY PROBE USING CROSS-CORRELATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; methods: data
   analysis; methods: statistical
ID BACKGROUND POWER SPECTRUM; WMAP OBSERVATIONS; 148 GHZ; GALAXY CLUSTERS;
   BEAM PROFILES; ARRAY CAMERA; 2003 FLIGHT; TEMPERATURE; MAPS;
   POLARIZATION
AB We present a new calibration method based on cross-correlations with the Wilkinson Microwave Anisotropy Probe (WMAP) and apply it to data from the Atacama Cosmology Telescope (ACT). ACT's observing strategy and map-making procedure allows an unbiased reconstruction of the modes in the maps over a wide range of multipoles. By directly matching the ACT maps to WMAP observations in the multipole range of 400 < l < 1000, we determine the absolute calibration with an uncertainty of 2% in temperature. The precise measurement of the calibration error directly impacts the uncertainties in the cosmological parameters estimated from the ACT power spectra. We also present a combined map based on ACT and WMAP data that has a high signal-to-noise ratio over a wide range of multipoles.
C1 [Hajian, Amir; Bond, John R.; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
   [Hajian, Amir; Acquaviva, Viviana; Das, Sudeep; Dunkley, Joanna; Lin, Yen-Ting; Lupton, Robert H.; Marriage, Tobias A.; Spergel, David N.; Trac, Hy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
   [Hajian, Amir; Appel, John William; Das, Sudeep; Dunkley, Joanna; Duenner, Rolando; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hincks, Adam D.; Lau, Judy M.; Limon, Michele; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
   [Acquaviva, Viviana; Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
   [Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
   [Aguirre, Paula; Felipe Barrientos, L.; Infante, Leopoldo; Baptiste Juin, Jean; Lin, Yen-Ting] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
   [Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
   [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
   [Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
   [Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
   [Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Marsden, Danica; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
   [Doriese, W. Bertrand; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
   [Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
   [Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany.
   [Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
   [Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa.
   [Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
   [Hughes, David H.] INAOE, Puebla, Mexico.
   [Lau, Judy M.; Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
   [Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
   [Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
   [Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
   [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
   [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
   [Reid, Beth] Univ Barcelona, ICREA, Barcelona 08028, Spain.
   [Reid, Beth] Univ Barcelona, ICC, Barcelona 08028, Spain.
   [Switzer, Eric R.] Kavli Inst Cosmol Phys, Lab Astrophys & Space Res, Chicago, IL 60637 USA.
   [Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
   [Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hajian, A (reprint author), Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew
   James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; 
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
   Huffenberger, Kevin/0000-0001-7109-0099; Sievers,
   Jonathan/0000-0001-6903-5074; Limon, Michele/0000-0002-5900-2698
FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
   PIRE-0507768]; Princeton University; University of Pennsylvania; Canada
   Foundation for Innovation under the auspices of Compute Canada;
   Government of Ontario; Ontario Research Fund-Research Excellence;
   University of Toronto; NASA [NNX08AH30G]; Natural Science and
   Engineering Research Council of Canada (NSERC); NSF [AST-0546035,
   AST-0606975]; FONDAP Centro de Astrofisica; CONICYT; MECESUP; Fundacion
   Andes; NSF Physics Frontier Center [PHY-0114422]; South African National
   Research Foundation (NRF); Meraka Institute; South African Square
   Kilometer Array (SKA) Project; RCUK; Berkeley Center for Cosmological
   Physics; World Premier International Research Center Initiative, MEXT,
   Japan; U.S. Department of Energy [DE-AC3-76SF00515]; NASA Office of
   Space Science
FX This work was supported by the U.S. National Science Foundation through
   awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731,
   and PIRE-0507768. Funding was also provided by Princeton University and
   the University of Pennsylvania. The PIRE program made possible exchanges
   between Chile, South Africa, Spain, and the United States that enabled
   this research program. Computations were performed on the GPC
   supercomputer at the SciNet HPC Consortium. SciNet is funded by the
   Canada Foundation for Innovation under the auspices of Compute Canada;
   the Government of Ontario; Ontario Research Fund-Research Excellence;
   and the University of Toronto.; A. H., V. A., S. D., and T. A. M. were
   supported through NASA grant NNX08AH30G. A. D. H. received additional
   support from a Natural Science and Engineering Research Council of
   Canada (NSERC) PGS-D scholarship. A. K. and B. P. were partially
   supported through NSF AST-0546035 and AST-0606975, respectively, for
   work on ACT. L. I. acknowledge partial support from FONDAP Centro de
   Astrofisica. R. D. was supported by CONICYT, MECESUP, and Fundacion
   Andes. E. R. S. acknowledges support by NSF Physics Frontier Center
   grant PHY-0114422 to the Kavli Institute of Cosmological Physics. K.M.,
   M. Hilton, and R. W. received financial support from the South African
   National Research Foundation (NRF), the Meraka Institute via funding for
   the South African Centre for High Performance Computing (CHPC), and the
   South African Square Kilometer Array (SKA) Project. J.D. received
   support from an RCUK Fellowship. R. H. received funding from the Rhodes
   Trust. We thank Norm Jarosik for useful discussions and his
   contributions. S.D. acknowledges support from the Berkeley Center for
   Cosmological Physics. Y.-T.L. acknowledges support from the World
   Premier International Research Center Initiative, MEXT, Japan. N.S. is
   supported by the U.S. Department of Energy contract to SLAC No.
   DE-AC3-76SF00515. We acknowledge the use of the Legacy Archive for
   Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is
   provided by the NASA Office of Space Science. The data will be made
   public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web
   site (http://www.physics.princeton.edu/act/). Some of the results in
   this paper have been derived using the HEALPix (Gorski et al. 2005)
   package.
NR 55
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
IS 2
AR 86
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PG 9
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SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900036
ER

PT J
AU Lynch, BJ
   Reinard, AA
   Mulligan, T
   Reeves, KK
   Rakowski, CE
   Allred, JC
   Li, Y
   Laming, JM
   MacNeice, PJ
   Linker, JA
AF Lynch, B. J.
   Reinard, A. A.
   Mulligan, T.
   Reeves, K. K.
   Rakowski, C. E.
   Allred, J. C.
   Li, Y.
   Laming, J. M.
   MacNeice, P. J.
   Linker, J. A.
TI IONIC COMPOSITION STRUCTURE OF CORONAL MASS EJECTIONS IN AXISYMMETRIC
   MAGNETOHYDRODYNAMIC MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; magnetohydrodynamics (MHD); Sun: corona; Sun:
   coronal mass ejections (CMEs); Sun: flares; Sun: heliosphere
ID INTER-PLANETARY SHOCK; SLOW SOLAR-WIND; CHARGE STATES;
   ELECTRON-TEMPERATURE; COMPOSITION SPECTROMETER; MAGNETIC-STRUCTURE; FLUX
   CANCELLATION; SOHO OBSERVATIONS; IONIZATION STATE; 1 AU
AB We present the ionic charge state composition structure derived from axisymmetric MHD simulations of coronal mass ejections (CMEs), initiated via the flux-cancellation and magnetic breakout mechanisms. The flux-cancellation CME simulation is run on the Magnetohydrodynamics-on-A-Sphere code developed at Predictive Sciences, Inc., and the magnetic breakout CME simulation is run on ARC7 developed at NASA GSFC. Both MHD codes include field-aligned thermal conduction, radiative losses, and coronal heating terms which make the energy equations sufficient to calculate reasonable temperatures associated with the steady-state solar wind and model the eruptive flare heating during CME formation and eruption. We systematically track a grid of Lagrangian plasma parcels through the simulation data and calculate the coronal density and temperature history of the plasma in and around the CME magnetic flux ropes. The simulation data are then used to integrate the continuity equations for the ionic charge states of several heavy ion species under the assumption that they act as passive tracers in the MHD flow. We construct two-dimensional spatial distributions of commonly measured ionic charge state ratios in carbon, oxygen, silicon, and iron that are typically elevated in interplanetary coronal mass ejection (ICME) plasma. We find that the slower CME eruption has relatively enhanced ionic charge states and the faster CME eruption shows basically no enhancement in charge states-which is the opposite trend to what is seen in the in situ ICME observations. The primary cause of the difference in the ionic charge states in the two simulations is not due to the different CME initiation mechanisms per se. Rather, the difference lies in their respective implementation of the coronal heating which governs the steady-state solar wind, density and temperature profiles, the duration of the connectivity of the CME to the eruptive flare current sheet, and the contribution of the flare-heated plasma associated with the reconnection jet outflow into the ejecta. Despite the limitations inherent in the first attempt at this novel procedure, the simulation results provide strong evidence in support of the conclusion that enhanced heavy ion charge states within CMEs are a direct consequence of flare heating in the low corona. We also discuss future improvements through combining numerical CME modeling with quantitative ionic charge state calculations.
C1 [Lynch, B. J.; Li, Y.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Reinard, A. A.] NOAA Space Weather Predict Ctr, Boulder, CO 80505 USA.
   [Mulligan, T.] Aerosp Corp, Dept Space Sci, Los Angeles, CA 90009 USA.
   [Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Rakowski, C. E.; Laming, J. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
   [Allred, J. C.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
   [MacNeice, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA.
RP Lynch, BJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM blynch@ssl.berkeley.edu; alysha.reinard@noaa.gov;
   tamitha.mulligan@aero.org; kreeves@cfa.harvard.edu;
   c.rakowski@nrl.navy.mil; jca32@drexel.edu; yanli@ssl.berkeley.edu;
   j.laming@nrl.navy.mil; peter.j.macneice@nasa.gov; linkerj@presci.com
RI Lynch, Benjamin/B-1300-2013; Reinard, Alysha/H-7808-2013; Reeves,
   Katharine/P-9163-2014; Allred, Joel/C-9550-2012; MacNeice,
   Peter/F-5587-2012
OI Reinard, Alysha/0000-0003-0304-2989; Lynch,
   Benjamin/0000-0001-6886-855X; 
FU NASA [HTP NNX08AI56G NNX11AJ65G, NASA HGI NNX08AJ04G, SRT NNX08AH54G,
   HGI NNG08EK62I, TRT NNG04GN00G]; Office of Naval Research; NSF [SHINE
   ATM0752257]
FX B.J.L. thanks S. K. Antiochos and G. H. Fisher for helpful discussion
   during the preparation of the manuscript. This collaborative research
   was made possible with support from NASA's Heliosphysics Theory, Guest
   Investigator, Living With a Star, and SR&T programs, as well as the NSF
   SHINE program, the Office of Naval Research, and the Center for
   Integrated Space Weather Modeling (an NSF Science and Technology
   Center). B.J.L. and Y.L. acknowledge support from NASA HTP NNX08AI56G
   NNX11AJ65G, and NASA HGI NNX08AJ04G; A.A.R. and T.L.M. acknowledge NASA
   SR&T NNX08AH54G; C.E.R. and J.M.L. acknowledge NASA HGI NNG08EK62I and
   basic research funds of the Office of Naval Research; K.K.R.
   acknowledges NSF SHINE ATM0752257; and J.C.A. and P.J.M. acknowledge
   support from NASA TR&T NNG04GN00G.
NR 86
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
IS 2
AR 112
DI 10.1088/0004-637X/740/2/112
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900062
ER

PT J
AU Meyer, ET
   Fossati, G
   Georganopoulos, M
   Lister, ML
AF Meyer, Eileen T.
   Fossati, Giovanni
   Georganopoulos, Markos
   Lister, Matthew L.
TI FROM THE BLAZAR SEQUENCE TO THE BLAZAR ENVELOPE: REVISITING THE
   RELATIVISTIC JET DICHOTOMY IN RADIO-LOUD ACTIVE GALACTIC NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: jets; galaxies: nuclei
ID BL-LACERTAE OBJECTS; FLAT-SPECTRUM SAMPLE; RAY BRIGHT BLAZARS; LAC
   UNIFYING MODEL; PARSEC-SCALE JET; FR-I; LUMINOSITY FUNCTION; TEV
   BLAZARS; OPTICAL SPECTROSCOPY; ENERGY-DISTRIBUTIONS
AB We revisit the concept of a blazar sequence that relates the synchrotron peak frequency (nu(peak)) in blazars with synchrotron peak luminosity (L-peak, in nu L-nu) using a large sample of radio-loud active galactic nuclei. We present observational evidence that the blazar sequence is formed from two populations in the synchrotron nu(peak)-L-peak plane, each forming an upper edge to an envelope of progressively misaligned blazars, and connecting to an adjacent group of radio galaxies having jets viewed at much larger angles to the line of sight. When binned by jet kinetic power (L-kin; as measured through a scaling relationship with extended radio power), we find that radio core dominance decreases with decreasing synchrotron L-peak, revealing that sources in the envelope are generally more misaligned. We find population-based evidence of velocity gradients in jets at low kinetic powers (similar to 10(42)-10(44.5) erg s(-1)), corresponding to Fanaroff-Riley (FR) I radio galaxies and most BL Lac objects. These low jet power "weak-jet" sources, thought to exhibit radiatively inefficient accretion, are distinguished from the population of non-decelerating, low synchrotron-peaking (LSP) blazars and FR II radio galaxies ("strong" jets) which are thought to exhibit radiatively efficient accretion. The two-population interpretation explains the apparent contradiction of the existence of highly core-dominated, low-power blazars at both low and high synchrotron peak frequencies, and further implies that most intermediate synchrotron peak sources are not intermediate in intrinsic jet power between LSP and high synchrotron-peaking (HSP) sources, but are more misaligned versions of HSP sources with similar jet powers.
C1 [Meyer, Eileen T.; Fossati, Giovanni] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
   [Georganopoulos, Markos] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
   [Georganopoulos, Markos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Lister, Matthew L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
RP Meyer, ET (reprint author), Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
EM meyer@rice.edu
RI Fossati, Giovanni/A-5841-2009
FU National Aeronautics and Space Administration [NNG05GJ10G, NNX06AE92G,
   NNX09AR04G, NNX08AG77G, NNX09AR88G]; SAO [GO3-4147X, G05-6115X];
   National Science Foundation [0807860-AST]
FX The authors wish to thank the anonymous referee for helpful comments,
   and Katherine Blundell for a discussion which lead to the improvement of
   this manuscript. This research has made use of the SIMBAD database,
   operated at CDS, Strasbourg, France
   (http://simbad.u-strasbg.fr/simbad/), and 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 (http://nedwww.ipac.caltech.edu/).
   We utilized package np (Hayfield & Racine 2008) in the R language and
   environment for statistical computing (R Development Core Team 2010).
   G.F. and E.M. acknowledge support from NASA grants NNG05GJ10G,
   NNX06AE92G, and NNX09AR04G, as well as SAO grants GO3-4147X and
   G05-6115X. M.G. acknowledges support from the NASA ATFP grant NNX08AG77G
   and NASA Fermi grant NNX09AR88G. The MOJAVE project is supported under
   National Science Foundation grant 0807860-AST.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
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SC Astronomy & Astrophysics
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ER

PT J
AU Milligan, RO
AF Milligan, Ryan O.
TI SPATIALLY RESOLVED NONTHERMAL LINE BROADENING DURING THE IMPULSIVE PHASE
   OF A SOLAR FLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: chromosphere; Sun: flares; Sun: UV radiation; Sun:
   X-rays, gamma rays
ID X-RAY-SPECTRA; GENTLE CHROMOSPHERIC EVAPORATION; EUV IMAGING
   SPECTROMETER; HIGH TIME RESOLUTION; ACTIVE-REGION; EXTREME-ULTRAVIOLET;
   EMISSION-LINES; ELEMENTS HYDROGEN; DENSITY STRUCTURE; RATE COEFFICIENTS
AB This paper presents a detailed study of excess line broadening in extreme ultraviolet (EUV) emission lines during the impulsive phase of a C-class solar flare. In this work, which utilizes data from the EUV Imaging Spectrometer on board Hinode, the broadened line profiles were observed to be cospatial with the two hard X-ray footpoints as observed by RHESSI. By plotting the derived nonthermal velocity for each pixel within the Fe XV and Fe XVI rasters against its corresponding Doppler velocity a strong correlation (vertical bar r vertical bar > 0.59) was found between the two parameters for one of the footpoints. This suggested that the excess broadening at these temperatures is due to a superposition of flows (turbulence), presumably as a result of chromospheric evaporation due to nonthermal electrons. Also presented are diagnostics of electron densities using five pairs of density-sensitive line ratios. Density maps derived using the Mg VII and Si X line pairs showed no appreciable increase in electron density at the footpoints, whereas the Fe XII, Fe XIII, and Fe XIV line pairs revealed densities approaching 10(11.5) cm(-3). Using this information, the nonthermal velocities derived from the widths of the two Fe XIV lines were plotted against their corresponding density values derived from their ratio. This showed that pixels with large nonthermal velocities were associated with pixels of moderately higher densities. This suggests that nonthermal broadening at these temperatures may have been due to enhanced densities at the footpoints, although estimates of the amount of opacity broadening and pressure broadening appeared to be negligible.
C1 [Milligan, Ryan O.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab Code 671, Greenbelt, MD 20771 USA.
RP Milligan, RO (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland.
FU Queen's University Belfast
FX The author thank Peter Young for his assistance with the density
   diagnostics and for feedback on the manuscript, Brian Dennis and Gordon
   Holman for their insightful and stimulating discussions, Mihalis
   Mathioudakis and Francis Keenan for discussions on opacity, the
   anonymous referee for their constructive comments, the International
   Space Science Institute (ISSI, Bern) for the opportunity to discuss
   these results at the international team meeting on chromospheric flares,
   and Queen's University Belfast for the award of a Leverhulme Trust
   Research Fellowship. Hinode is a Japanese mission developed and launched
   by ISAS/JAXA, collaborating with NAOJ as domestic partner, and NASA
   (USA) and STFC (UK) as international partners. Scientific operation of
   the Hinode mission is conducted by the Hinode science team organized at
   ISAS/JAXA. This team mainly consists of scientists from institutes in
   the partner countries. Support for the post-launch operation is provided
   by JAXA and NAOJ, STFC, NASA, ESA (European Space Agency), and NSC
   (Norway).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
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SC Astronomy & Astrophysics
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UT WOS:000296762900020
ER

PT J
AU Moran, TG
AF Moran, Thomas G.
TI RADIATIVE HEATING OF THE SOLAR CORONA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun: atmosphere; Sun: chromosphere; Sun: corona; Sun:
   fundamental parameters; Sun: heliosphere
ID IMAGING SPECTROMETER OBSERVATIONS; ACTIVE-REGION; QUIET SUN; SOHO;
   YOHKOH; PLASMAS; HINODE; MODELS; TRACE; SUMER
AB We investigate the effect of solar visible and infrared radiation on electrons in the Sun's atmosphere using a Monte Carlo simulation of the wave-particle interaction and conclude that sunlight provides at least 40% and possibly all of the power required to heat the corona, with the exception of dense magnetic flux loops. The simulation uses a radiation waveform comprising 100 frequency components spanning the solar blackbody spectrum. Coronal electrons are heated in a stochastic manner by low coherence solar electromagnetic radiation. The wave "coherence time" and "coherence volume" for each component is determined from optical theory. The low coherence of solar radiation allows moving electrons to gain energy from the chaotic wave field which imparts multiple random velocity "kicks" to these particles causing their velocity distribution to broaden or heat. Monte Carlo simulations of broadband solar radiative heating on ensembles of 1000 electrons show heating at per particle levels of 4.0 x 10(-21) to 4.0 x 10(-20) W, as compared with non-loop radiative loss rates of approximate to 1 x 10(-20) W per electron. Since radiative losses comprise nearly all of the power losses in the corona, sunlight alone can explain the elevated temperatures in this region. The volume electron heating rate is proportional to density, and protons are assumed to be heated either by plasma waves or through collisions with electrons.
C1 [Moran, Thomas G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Moran, Thomas G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Moran, TG (reprint author), Catholic Univ Amer, Dept Phys, 200 Hannan Hall, Washington, DC 20064 USA.
EM moran@grace.nascom.nasa.gov
NR 29
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
IS 2
AR 62
DI 10.1088/0004-637X/740/2/62
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900012
ER

PT J
AU Ofek, EO
   Frail, DA
   Breslauer, B
   Kulkarni, SR
   Chandra, P
   Gal-Yam, A
   Kasliwal, MM
   Gehrels, N
AF Ofek, E. O.
   Frail, D. A.
   Breslauer, B.
   Kulkarni, S. R.
   Chandra, P.
   Gal-Yam, A.
   Kasliwal, M. M.
   Gehrels, N.
TI A VERY LARGE ARRAY SEARCH FOR 5 GHz RADIO TRANSIENTS AND VARIABLES AT
   LOW GALACTIC LATITUDES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radio continuum: general; stars: neutron; techniques: photometric
ID GAMMA-RAY-BURST; REFRACTIVE INTERSTELLAR SCINTILLATION; LOW-FREQUENCY
   VARIABILITY; NORTHERN MILKY-WAY; WIDE-FIELD SURVEY; SKY SURVEY;
   NEUTRON-STARS; CATALOG; TELESCOPE; PLANE
AB We present the results of a 5 GHz survey with the Very Large Array (VLA) and the expanded VLA, designed to search for short-lived (less than or similar to 1 day) transients and to characterize the variability of radio sources at milli-Jansky levels. A total sky area of 2.66 deg(2), spread over 141 fields at low Galactic latitudes (b congruent to 6-8 deg), was observed 16 times with a cadence that was chosen to sample timescales of days, months, and years. Most of the data were reduced, analyzed, and searched for transients in near real-time. Interesting candidates were followed up using visible light telescopes (typical delays of 1-2 hr) and the X-ray Telescope on board the Swift satellite. The final processing of the data revealed a single possible transient with a peak flux density of f(nu) congruent to 2.4 mJy. This implies a transient's sky surface density of kappa(f(nu) > 1.8mJy) = 0.039(-0.032,-0.038)(+0.13,+0.18) deg(-2) (1 sigma, 2 sigma confidence errors). This areal density is roughly consistent with the sky surface density of transients from the Bower et al. survey extrapolated to 1.8 mJy. Our observed transient areal density is consistent with a neutron star's origin for these events. Furthermore, we use the data to measure the source variability on timescales of days to years, and we present the variability structure function of 5 GHz sources. The mean structure function shows a fast increase on approximate to 1 day timescale, followed by a slower increase on timescales of up to 10 days. On timescales between 10 and 60 days, the structure function is roughly constant. We find that greater than or similar to 30% of the unresolved sources brighter than 1.8 mJy are variables at the >4 sigma confidence level, presumably mainly due to refractive scintillation.
C1 [Ofek, E. O.; Kulkarni, S. R.; Kasliwal, M. M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
   [Frail, D. A.; Breslauer, B.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
   [Breslauer, B.] Oberlin Coll, Dept Phys & Astron, Oberlin, OH 44074 USA.
   [Chandra, P.] Royal Mil Coll Canada, Dept Phys, Kingston, ON, Canada.
   [Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
   [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ofek, EO (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
RI Gehrels, Neil/D-2971-2012
FU Einstein fellowship; NASA [NAS5-26555]; NASA through Space Telescope
   Science Institute [HST-GO-11104.01-A]; Israeli Science Foundation; EU;
   Benoziyo Center for Astrophysics; Weizmann Institute
FX We are grateful to Barry Clark for his help with scheduling the VLA
   observations. We thank the anonymous referee for useful comments. E.O.O.
   is supported by an Einstein fellowship and NASA grants. Support for
   program number HST-GO-11104.01-A was provided by NASA through a grant
   from the Space Telescope Science Institute, which is operated by the
   Association of Universities for Research in Astronomy, Incorporated,
   under NASA contract NAS5-26555. A.G. acknowledges support by the Israeli
   Science Foundation, an EU Seventh Framework Programme Marie Curie IRG
   fellowship, the Benoziyo Center for Astrophysics, and the Yeda-Sela fund
   at the Weizmann Institute. This paper is based on observations conducted
   with the VLA, which is operated by the National Radio Astronomy
   Observatory (NRAO), a facility of the National Science Foundation
   operated under cooperative agreement by Associated Universities, Inc.
NR 84
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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 OCT 20
PY 2011
VL 740
IS 2
AR 65
DI 10.1088/0004-637X/740/2/65
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900015
ER

PT J
AU Tripathi, D
   Klimchuk, JA
   Mason, HE
AF Tripathi, Durgesh
   Klimchuk, James A.
   Mason, Helen E.
TI EMISSION MEASURE DISTRIBUTION AND HEATING OF TWO ACTIVE REGION CORES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: atmosphere; Sun: corona; Sun: transition region; Sun: UV radiation
ID ULTRAVIOLET IMAGING SPECTROMETER; CORONAL LOOPS; SOLAR CORONA;
   TRANSITION REGION; DENSITY STRUCTURE; ATOMIC DATABASE; RAY TELESCOPE;
   HOT PLASMA; HINODE; TRACE
AB Using data from the Extreme-ultraviolet Imaging Spectrometer aboard Hinode, we have studied the coronal plasma in the core of two active regions. Concentrating on the area between opposite polarity moss, we found emission measure distributions having an approximate power-law form EM proportional to T-2.4 from log T = 5.5 up to a peak at log T = 6.55. We show that the observations compare very favorably with a simple model of nanoflare-heated loop strands. They also appear to be consistent with more sophisticated nanoflare models. However, in the absence of additional constraints, steady heating is also a viable explanation.
C1 [Tripathi, Durgesh] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
   [Tripathi, Durgesh; Mason, Helen E.] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England.
   [Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Tripathi, D (reprint author), Interuniv Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India.
EM durgesh@iucaa.ernet.in
RI Klimchuk, James/D-1041-2012; Tripathi, Durgesh/D-9390-2012
OI Klimchuk, James/0000-0003-2255-0305; Tripathi,
   Durgesh/0000-0003-1689-6254
FU STFC; NASA
FX D.T. and H.E.M. acknowledge support from STFC. The work of J.A.K. was
   supported by the NASA Supporting Research and Technology and Living With
   a Star Programs. CHIANTI is a collaborative project involving
   researchers at NRL (USA), RAL (UK), and the Universities of Cambridge
   (UK), George Mason (USA), and Florence (Italy). We thank Dr. Giulio Del
   Zanna for various discussions and Dr. Peter Young for providing his
   softwares to Solarsoft. We also thank Dr. Amy Winebarger for providing
   constructive comments as a referee. Hinode is a Japanese mission
   developed and launched by ISAS/JAXA, collaborating with NAOJ as a
   domestic partner, NASA and STFC (UK) as international partners.
   Scientific operation of the Hinode mission is conducted by the Hinode
   science team organized at ISAS/JAXA. This team mainly consists of
   scientists from institutes in the partner countries. Support for the
   post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK),
   NASA, ESA, and NSC (Norway).
NR 48
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
IS 2
AR 111
DI 10.1088/0004-637X/740/2/111
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900061
ER

PT J
AU Fu, H
   Zhang, ZY
   Assef, RJ
   Stockton, A
   Myers, AD
   Yan, L
   Djorgovski, SG
   Wrobel, JM
   Riechers, DA
AF Fu, Hai
   Zhang, Zhi-Yu
   Assef, Roberto J.
   Stockton, Alan
   Myers, Adam D.
   Yan, Lin
   Djorgovski, S. G.
   Wrobel, J. M.
   Riechers, Dominik A.
TI A KILOPARSEC-SCALE BINARY ACTIVE GALACTIC NUCLEUS CONFIRMED BY THE
   EXPANDED VERY LARGE ARRAY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: individual (SDSS J150243.1+111557);
   galaxies: interactions; galaxies: nuclei
ID SUPERMASSIVE BLACK-HOLES; LINE REGION KINEMATICS; DIGITAL SKY SURVEY;
   RADIO-SOURCES; GALAXIES; QUASAR; LUMINOSITY; DISCOVERY; OBJECTS; SAMPLE
AB We report the confirmation of a kiloparsec-scale binary active galactic nucleus (AGN) with high-resolution radio images from the Expanded Very Large Array (EVLA). SDSS J150243.1+111557 is a double-peaked [O III] AGN at z = 0.39 selected from the Sloan Digital Sky Survey. Our previous near-infrared adaptive optics imaging reveals two nuclei separated by 1.'' 4 (7.4 kpc), and our optical integral-field spectroscopy suggests that they are a type-1-type-2 AGN pair. However, these data alone cannot rule out the single AGN scenario where the narrow emission-line region associated with the secondary is photoionized by the broad-line AGN in the primary. Our new EVLA images at 1.4, 5.0, and 8.5 GHz show two steep-spectrum compact radio sources spatially coincident with the optical nuclei. The radio power of the type-2 AGN is an order-of-magnitude in excess of star-forming galaxies with similar extinction-corrected [O II] lambda 3727 luminosities, indicating that the radio emission is powered by accretion. Therefore, SDSS J150243.1+111557 is one of the few confirmed kiloparsec-scale binary AGN systems. Spectral energy distribution modeling shows that SDSS J150243.1+111557 is a merger of two similar to 10(11) M-circle dot galaxies. With both black hole masses around 10(8) M-circle dot, the AGNs are accreting at similar to 10 times below the Eddington limit.
C1 [Fu, Hai; Djorgovski, S. G.; Riechers, Dominik A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
   [Zhang, Zhi-Yu] CAS, Purple Mt Observ, Nanjing 210008, Peoples R China.
   [Zhang, Zhi-Yu] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
   [Zhang, Zhi-Yu] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China.
   [Assef, Roberto J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Stockton, Alan] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
   [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
   [Myers, Adam D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Yan, Lin] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
   [Wrobel, J. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Fu, H (reprint author), CALTECH, Dept Astron, MS 249-17, Pasadena, CA 91125 USA.
OI Zhang, Zhiyu/0000-0002-7299-2876
FU NSFC [10833006]; NSF [AST-0807900, AST-0909182]; Ajax Foundation
FX Z.Y.Z. acknowledges support by NSFC key project 10833006. A. D. M. is a
   research fellow of the Alexander von Humboldt Foundation of Germany. A.
   S. and S. G. D. were partially supported by NSF grants AST-0807900 and
   AST-0909182, respectively. S. G. D. also acknowledges support by the
   Ajax Foundation. The National Radio Astronomy Observatory is a facility
   of the National Science Foundation operated under cooperative agreement
   by Associated Universities, Inc.
NR 49
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2011
VL 740
IS 2
AR L44
DI 10.1088/2041-8205/740/2/L44
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844MZ
UT WOS:000296752600013
ER

PT J
AU Ofman, L
   Liu, W
   Title, A
   Aschwanden, M
AF Ofman, L.
   Liu, W.
   Title, A.
   Aschwanden, M.
TI MODELING SUPER-FAST MAGNETOSONIC WAVES OBSERVED BY SDO IN ACTIVE REGION
   FUNNELS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE magnetohydrodynamics (MHD); Sun: activity; Sun: corona; Sun: coronal
   mass ejections (CMEs); Sun: flares; Sun: oscillations; Sun: UV
   radiation; waves
ID ULTRAVIOLET IMAGING TELESCOPE; SOLAR CORONA; NUMERICAL-SIMULATION; EIT
   WAVES; OSCILLATIONS; STEREO; LOOPS
AB Recently, quasi-periodic, rapidly propagating waves have been observed in extreme ultraviolet by the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA) instrument in about 10 flare/coronal mass ejection (CME) events thus far. A typical example is the 2010 August 1 C3.2 flare/CME event that exhibited arc-shaped wave trains propagating in an active region (AR) magnetic funnel with similar to 5% intensity variations at speeds in the range of 1000-2000 km s(-1). The fast temporal cadence and high sensitivity of AIA enabled the detection of these waves. We identify them as fast magnetosonic waves driven quasi-periodically at the base of the flaring region and develop a three-dimensional MHD model of the event. For the initial state we utilize the dipole magnetic field to model the AR and include gravitationally stratified density at coronal temperature. At the coronal base of the AR, we excite the fast magnetosonic wave by periodic velocity pulsations in the photospheric plane confined to a funnel of magnetic field lines. The excited fast magnetosonic waves have similar amplitude, wavelength, and propagation speeds as the observed wave trains. Based on the simulation results, we discuss the possible excitation mechanism of the waves, their dynamical properties, and the use of the observations for coronal MHD seismology.
C1 [Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Ofman, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Liu, W.; Title, A.; Aschwanden, M.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
   [Liu, W.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RP Ofman, L (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel.
FU NASA [NNX08AV88G, NNX09AG10G]; AIA [NNG04EA00C]; NASA through the NASA
   Advanced Supercomputing (NAS) Division at Ames Research Center
FX We are grateful to the SDO/AIA team for providing the data used in this
   study. L.O. was supported by NASA Grants NNX08AV88G and NNX09AG10G. W.
   L. was supported by AIA Contract NNG04EA00C. Resources supporting this
   work were provided by the NASA High-End Computing (HEC) Program through
   the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
NR 25
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2011
VL 740
IS 2
AR L33
DI 10.1088/2041-8205/740/2/L33
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844MZ
UT WOS:000296752600002
ER

PT J
AU Sahai, R
   Neill, JD
   de Paz, AG
   Contreras, CS
AF Sahai, Raghvendra
   Neill, James D.
   Gil de Paz, Armando
   Sanchez Contreras, Carmen
TI STRONG VARIABLE ULTRAVIOLET EMISSION FROM Y GEM: ACCRETION ACTIVITY IN
   AN ASYMPTOTIC GIANT BRANCH STAR WITH A BINARY COMPANION?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; binaries: general; circumstellar matter;
   stars: AGB and post-AGB; stars: individual (Y Gem, Mira); stars:
   mass-loss
ID MORPHOLOGICAL CLASSIFICATION-SYSTEM; T-TAURI STARS; PLANETARY-NEBULAE;
   WIND-ACCRETION; SPECTRA; CATALOG; FLARE; SHOCK; CO
AB Binarity is believed to dramatically affect the history and geometry of mass loss in asymptotic giant branch (AGB) and post-AGB stars, but observational evidence of binarity is sorely lacking. As part of a project to look for hot binary companions to cool AGB stars using the Galaxy Evolution Explorer archive, we have discovered a late-M star, Y Gem, to be a source of strong and variable UV emission. Y Gem is a prime example of the success of our technique of UV imaging of AGB stars in order to search for binary companions. Y Gem's large and variable UV flux makes it one of the most prominent examples of a late-AGB star with a mass accreting binary companion. The UV emission is most likely due to emission associated with accretion activity and a disk around a main-sequence companion star. The physical mechanism generating the UV emission is extremely energetic, with an integrated luminosity of a few x L-circle dot at its peak. We also find weak CO J = 2-1 emission from Y Gem with a very narrow line profile (FWHM of 3.4 km s(-1)). Such a narrow line is unlikely to arise in an outflow and is consistent with emission from an orbiting, molecular reservoir of radius 300 AU. Y Gem may be the progenitor of the class of post-AGB stars which are binaries and possess disks but no outflows.
C1 [Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Neill, James D.] CALTECH, Pasadena, CA 91125 USA.
   [Gil de Paz, Armando] Univ Complutense Madrid, Dpto Astrofis, E-28040 Madrid, Spain.
   [Sanchez Contreras, Carmen] Astrobiol Ctr CSIC INTA, E-28691 Madrid, Spain.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
RI Sanchez-Contreras, Carmen/N-3718-2015; Gil de Paz, Armando/J-2874-2016
OI Sanchez-Contreras, Carmen/0000-0002-6341-592X; Gil de Paz,
   Armando/0000-0001-6150-2854
FU NASA; GALEX
FX We thank the staff of the Arizona Radio Observatory for granting us
   observing time. We thank Noam Soker and Joel Kastner for their valuable
   comments on an earlier version of this Letter. R.S.'s contribution to
   the research described here was carried out at the Jet Propulsion
   Laboratory, California Institute of Technology, under a contract with
   NASA. Financial support was provided by NASA through a Long Term Space
   Astrophysics and GALEX GO award.
NR 35
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2011
VL 740
IS 2
AR L39
DI 10.1088/2041-8205/740/2/L39
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844MZ
UT WOS:000296752600008
ER

PT J
AU Tanaka, T
   Allafort, A
   Ballet, J
   Funk, S
   Giordano, F
   Hewitt, J
   Lemoine-Goumard, M
   Tajima, H
   Tibolla, O
   Uchiyama, Y
AF Tanaka, T.
   Allafort, A.
   Ballet, J.
   Funk, S.
   Giordano, F.
   Hewitt, J.
   Lemoine-Goumard, M.
   Tajima, H.
   Tibolla, O.
   Uchiyama, Y.
TI GAMMA-RAY OBSERVATIONS OF THE SUPERNOVA REMNANT RX J0852.0-4622 WITH THE
   FERMI LARGE AREA TELESCOPE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; gamma rays: ISM; ISM: individual objects (RX
   J0852.0, 4622); ISM: supernova remnants; radiation mechanisms:
   non-thermal
ID COMPACT CENTRAL OBJECT; PARTICLE-ACCELERATION; NORTHWESTERN RIM;
   CASSIOPEIA-A; VELA JR; RX-J0852.0-4622; EMISSION; J1713.7-3946;
   G266.2-1.2; TEV
AB We report on gamma-ray observations of the supernova remnant (SNR) RX J0852.0-4622 with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. In the Fermi-LAT data, we find a spatially extended source at the location of the SNR. The extension is consistent with the SNR size seen in other wavelengths such as X-rays and TeV gamma rays, leading to the identification of the gamma-ray source with the SNR. The spectrum is well described as a power law with a photon index of Gamma = 1.85 +/- 0.06 (stat)(-0.19)(+0.18) (sys), which smoothly connects to the H. E. S. S. spectrum in the TeV energy band. We discuss the gamma-ray emission mechanism based on multiwavelength data. The broadband data can be fit well by a model in which the gamma rays are of hadronic origin. We also consider a scenario with inverse Compton scattering of electrons as the emission mechanism of the gamma rays. Although the leptonic model predicts a harder spectrum in the Fermi-LAT energy range, the model can fit the data considering the statistical and systematic errors.
C1 [Tanaka, T.; Allafort, A.; Funk, S.; Tajima, H.; Uchiyama, Y.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
   [Tanaka, T.; Allafort, A.; Funk, S.; Tajima, H.; Uchiyama, Y.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
   [Ballet, J.] Univ Paris Diderot, CEA Saclay, Lab AIM, Serv Astrophys,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France.
   [Giordano, F.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
   [Giordano, F.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
   [Hewitt, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Lemoine-Goumard, M.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France.
   [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
   [Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
RP Tanaka, T (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
EM Taka.Tanaka@stanford.edu
RI Funk, Stefan/B-7629-2015; 
OI Funk, Stefan/0000-0002-2012-0080; Giordano,
   Francesco/0000-0002-8651-2394
FU European Community [ERC-StG-259391]
FX Funded by Contract ERC-StG-259391 from the European Community.; The
   Fermi-LAT Collaboration acknowledges support from a number of agencies
   and institutes for both development and the operation of LAT as well as
   scientific data analysis. These include NASA and DOE in the United
   States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT,
   KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish
   Research Council, and the National Space Board in Sweden. Additional
   support from INAF in Italy and CNES in France for science analysis
   during the operations phase is also gratefully acknowledged.
NR 32
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2011
VL 740
IS 2
AR L51
DI 10.1088/2041-8205/740/2/L51
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844MZ
UT WOS:000296752600020
ER

PT J
AU Tappa, MJ
   Coleman, DS
   Mills, RD
   Samperton, KM
AF Tappa, Michael J.
   Coleman, Drew S.
   Mills, Ryan D.
   Samperton, Kyle M.
TI The plutonic record of a silicic ignimbrite from the Latir volcanic
   field, New Mexico
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE pluton-ignimbrite connections
ID RIO-GRANDE RIFT; U-PB GEOCHRONOLOGY; NORTHERN NEW-MEXICO; QUESTA
   CALDERA; INTRUSIVE SUITE; MAGMA CHAMBERS; LONG VALLEY; EMPLACEMENT;
   ZIRCON; CALIFORNIA
AB Zircon U-Pb geochronologic data for plutonic rocks in the Latir volcanic field, New Mexico, demonstrate that the rocks are dominated by plutons that post-date ignimbrite eruption. Only zircon from the ring dike of the Questa caldera yields the same age (25.64 +/- 0.08 Ma) as zircon from the caldera-forming Amalia Tuff (25.52 +/- 0.06 Ma). The post-caldera Rio Hondo pluton was assembled incrementally over at least 400 ka. The magma accumulation rate for the exposed portion of the Rio Hondo pluton is estimated to be 0.0003 km(3) a(-1), comparable to rates for other plutons, and too slow to support accumulation of large eruptible magma volumes. Extrapolation of the accumulation rate for the Rio Hondo pluton over the history of the Latir volcanic field yields an estimated volume of plutonic rocks comparable to the calculated volume under the field as determined by geophysical studies. We propose that the bulk of the plutonic rocks beneath the volcanic center accumulated during periods of low volcanic effusivity. Furthermore, because the oldest portion of the Rio Hondo pluton is the granitic cap exposed beneath a gently dipping roof contact, the roof granite cannot be a silicic liquid fractionated from the deeper (younger) portions of the pluton. Instead, our data suggest that the compositional heterogeneity of the Rio Hondo pluton is inherited from lower crustal sources. We suggest that if magma fluxes are high enough, zoned ignimbrites can be formed by evolution of the melt compositions generated at the source with little or no shallow crustal differentiation.
C1 [Tappa, Michael J.; Coleman, Drew S.; Mills, Ryan D.; Samperton, Kyle M.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA.
RP Tappa, MJ (reprint author), NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA.
EM dcoleman@unc.edu
RI Samperton, Kyle/K-9286-2015
OI Samperton, Kyle/0000-0003-0177-5978
FU UNC; USGS through Ren Thompson; Sigma Xi; Dunlevie Undergraduate Honors
   Research Fund; UNC Honors Office
FX Tappa and Mills received funding from the UNC Martin fund. Tappa also
   received funding from the USGS through Ren Thompson in support of field
   research. Mills received funding from Sigma Xi, and Samperton received
   funding from the Dunlevie Undergraduate Honors Research Fund, UNC Honors
   Office. Field work could not have been conducted without the help of
   collaborator Matt Zimmerer. Peter Lipman and Allen Glazner reviewed
   early versions of this manuscript. Journal reviews by Shan de Silva,
   Mark Schmitz, and an anonymous reviewer significantly improved the
   quality and clarity of the manuscript. The ideas in this manuscript
   benefited tremendously from discussions with Peter Lipman, Matt
   Zimmerer, Bill McIntosh, Allen Glazner, John Bartley, Jesse Davis and
   Jan Tympel, though they may individually agree with few of the
   discussion points, interpretations or conclusions. Jesse Davis and John
   Gracely helped tremendously with the laboratory work.
NR 71
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U1 1
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD OCT 20
PY 2011
VL 12
AR Q10011
DI 10.1029/2011GC003700
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 836XA
UT WOS:000296150100001
ER

PT J
AU Abe, M
   Taguchi, S
   Collier, MR
   Moore, TE
AF Abe, M.
   Taguchi, S.
   Collier, M. R.
   Moore, T. E.
TI Two azimuthally separated regions of cusp ion injection observed via
   energetic neutral atoms
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; NORTHWARD IMF; ELECTRIC-FIELD;
   SOLAR-WIND; MAGNETOPAUSE MOTION; IMAGE SPACECRAFT; ALIGNED CURRENTS;
   LOW-LATITUDE; POLAR CUSP; CONVECTION
AB The low-energy neutral atom (LENA) imager on the IMAGE spacecraft can detect energetic neutral atoms produced by ion injection into the cusp through a charge exchange with the Earth's hydrogen exosphere. We examined the occurrence of the LENA cusp signal during positive IMF B-Z in terms of the arrival direction and the IMF clock angle theta(CA). Results of statistical analyses show that the occurrence frequency is high on the postnoon side when theta(CA) is between similar to 20 degrees and similar to 50 degrees. This is ascribed to ion injection caused by cusp reconnection typical of positive IMF B-Z. Our results also show that there is another situation of high occurrence frequency, which can be identified with theta(CA) of similar to 30 degrees to similar to 80 degrees. When theta(CA) is relatively large (60 degrees-80 degrees), occurrence frequencies are high at relatively low latitudes over a wide extent spanning both prenoon and postnoon sectors. This feature suggests that the ion injection is caused by reconnection at the dayside magnetopause. Its postnoon side boundary shifts toward the prenoon as theta(CA) decreases. When theta(CA) is less than similar to 50 degrees, the high occurrence frequency exists well inside the prenoon sector, which is azimuthally separated from the postnoon region ascribed to cusp reconnection. The prenoon region, which is thought due to ion injection caused by dayside reconnection, may explain the recent report that proton aurora brightening occurs in the unanticipated prenoon sector of the northern high-latitude ionosphere for IMF B-Y > 0 and B-Z > 0.
C1 [Abe, M.; Taguchi, S.] Univ Electrocommun, Dept Commun Engn & Informat, Tokyo 1828585, Japan.
   [Collier, M. R.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Taguchi, S.] Univ Electrocommun, Ctr Space Sci & Radio Engn, Tokyo 1828585, Japan.
RP Abe, M (reprint author), Univ Electrocommun, Dept Commun Engn & Informat, Tokyo 1828585, Japan.
EM taguchi@ice.uec.ac.jp
RI Moore, Thomas/D-4675-2012; Collier, Michael/I-4864-2013
OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605
FU Japan Society for the Promotion of Science [22340143]
FX This work was supported in part by Grant-in-Aid for Scientific Research
   (B) 22340143 under Japan Society for the Promotion of Science. M. Abe
   would like to thank K. Hosokawa for valuable discussion. ACE magnetic
   field and plasma data were provided by N. Ness and D. McComas through
   the NASA CDAWeb.
NR 54
TC 1
Z9 1
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 20
PY 2011
VL 116
AR A10225
DI 10.1029/2011JA016778
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 836ZG
UT WOS:000296158400006
ER

PT J
AU MacNeice, P
   Elliott, B
   Acebal, A
AF MacNeice, Peter
   Elliott, Brian
   Acebal, Ariel
TI Validation of community models: 3. Tracing field lines in heliospheric
   models
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID ENERGETIC PARTICLE EVENTS; SOLAR MAGNETIC-FIELD; WIND SPEED; ABUNDANCES;
   TRANSPORT; ORIGIN; FLARES; CORONA; SUN
AB Forecasting hazardous gradual solar energetic particle (SEP) bursts at Earth requires accurately modeling field line connections between Earth and the locations of coronal or interplanetary shocks that accelerate the particles. We test the accuracy of field lines reconstructed using four different models of the ambient coronal and inner heliospheric magnetic field, through which these shocks must propagate, including the coupled Wang-Sheeley-Arge (WSA)/ENLIL model. Evaluating the WSA/ENLIL model performance is important since it is the most sophisticated model currently available to space weather forecasters which can model interplanetary coronal mass ejections and, when coupled with particle acceleration and transport models, will provide a complete model for gradual SEP bursts. Previous studies using a simpler Archimedean spiral approach above 2.5 solar radii have reported poor performance. We test the accuracy of the model field lines connecting Earth to the Sun at the onset times of 15 impulsive SEP bursts, comparing the foot points of these field lines with the locations of surface events believed to be responsible for the SEP bursts. We find the WSA/ENLIL model performance is no better than the simplest spiral model, and the principal source of error is the model's inability to reproduce sufficient low-latitude open flux. This may be due to the model's use of static synoptic magnetograms, which fail to account for transient activity in the low corona, during which reconnection events believed to initiate the SEP acceleration may contribute short-lived open flux at low latitudes. Time-dependent coronal models incorporating these transient events may be needed to significantly improve Earth/Sun field line forecasting.
C1 [MacNeice, Peter] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Elliott, Brian; Acebal, Ariel] USAF, Dept Engn Phys, Inst Technol, Wright Patterson AFB, OH 45433 USA.
RP MacNeice, P (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
EM Peter.J.MacNeice@nasa.gov
NR 28
TC 12
Z9 12
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD OCT 20
PY 2011
VL 9
AR S10003
DI 10.1029/2011SW000665
PG 15
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
GA 837AE
UT WOS:000296161800001
ER

PT J
AU Gengeliczki, Z
   Callahan, MP
   Kabelac, M
   Rijs, AM
   de Vries, MS
AF Gengeliczki, Zsolt
   Callahan, Michael P.
   Kabelac, Martin
   Rijs, Anouk M.
   de Vries, Mattanjah S.
TI Structure of 2,4-Diaminopyrimidine-Theobromine Alternate Base Pairs
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID AB-INITIO CALCULATIONS; DOUBLE-RESONANCE SPECTROSCOPY; BASIS-SET;
   GUANINE; CYTOSINE; NUCLEOBASES; SELECTIVITY; MOLECULES; DYNAMICS
AB We report the structure of dusters of 2,4-diaminopyrimidine with 3,7-dimethylxanthine (theobromine) in the gas phase determined by IR-UV double resonance spectroscopy in both the near-IR and mid-IR regions in combination with ab initio computations. These clusters represent potential alternate nucleobase pairs, geometrically equivalent to guanine cytosine. We have found the four lowest energy structures, which include the Watson Crick base pairing motif. This Watson Crick structure has not been observed by resonant two-photon ionization (R2PI) in the gas phase for the canonical DNA base pairs.
C1 [de Vries, Mattanjah S.] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA.
   [Gengeliczki, Zsolt] Stanford Univ, Dept Chem, Stanford, CA 94305 USA.
   [Callahan, Michael P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Kabelac, Martin] Univ S Bohemia, Fac Nat Sci, Ceske Budejovice 37005, Czech Republic.
   [Kabelac, Martin] Acad Sci Czech Republic, Inst Organ Chem & Biochem, Vvi, Ctr Biomol & Complex Mol Syst, CR-16610 Prague 6, Czech Republic.
   [Rijs, Anouk M.] FOM Inst Plasma Phys Rijnhuizen, NL-3439 MN Nieuwegein, Netherlands.
RP de Vries, MS (reprint author), Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA.
EM devries@chem.ucsb.edu
RI Callahan, Michael/D-3630-2012; Rijs, Anouk/D-6536-2012; Kabelac,
   Martin/D-7206-2016
OI Rijs, Anouk/0000-0002-7446-9907; Kabelac, Martin/0000-0002-0518-5900
FU National Science Foundation [CHE-0911564]; Institute of Organic
   Chemistry and Biochemistry, Academy of Sciences of the Czech Republic
   [Z40550506]; Ministry of Education, Youth and Sports, Czech Republic
   [LC512]; Grant Agency of the Academy of Sciences of the Czech Republic
   [IAA400550808]; Borchard Foundation
FX This material is based upon work supported by the National Science
   Foundation under CHE-0911564. The skillful assistance of the FELIX staff
   is gratefully acknowledged. This work was a part of the research project
   No. Z40550506 of the Institute of Organic Chemistry and Biochemistry,
   Academy of Sciences of the Czech Republic and it was supported by Grants
   LC512 (Ministry of Education, Youth and Sports, Czech Republic) and No.
   IAA400550808 (Grant Agency of the Academy of Sciences of the Czech
   Republic).] MSdV thanks the Borchard Foundation for a Scholarship in
   Residence.
NR 25
TC 6
Z9 6
U1 2
U2 16
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD OCT 20
PY 2011
VL 115
IS 41
BP 11423
EP 11427
DI 10.1021/jp205831n
PG 5
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 831AH
UT WOS:000295700600034
PM 21888324
ER

PT J
AU Saito, MH
   Fairfield, D
   Le, G
   Hau, LN
   Angelopoulos, V
   McFadden, JP
   Auster, U
   Bonnell, JW
   Larson, D
AF Saito, M. H.
   Fairfield, D.
   Le, G.
   Hau, L. -N.
   Angelopoulos, V.
   McFadden, J. P.
   Auster, U.
   Bonnell, J. W.
   Larson, D.
TI Structure, force balance, and evolution of incompressible cross-tail
   current sheet thinning
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SUBSTORM GROWTH-PHASE; EARTH PLASMA SHEET; BALLOONING INSTABILITY;
   LOW-FREQUENCY; MAGNETOTAIL; ONSET; THEMIS; CONFIGURATION; INSTRUMENT;
   CONVECTION
AB THEMIS five-point observations on April 8, 2009 were used to study thinning of the current sheet in the near-Earth tail that led to the onset of a small substorm. Taking advantage of a fortuitous alignment of the five spacecraft near 2300 LT and 11 R-E and within 1.5 R-E of the current sheet center, latitudinal gradients are analyzed. A significant latitudinal pressure gradient is present indicating the necessity of a (J x B)(z) force to maintain the pre-onset equilibrium state. During thinning the total pressure remained approximately constant at all spacecraft rather than increasing. Within the plasma sheet, magnetic field strength increased while plasma pressure decreased due to decreasing temperature. We present a comprehensive explanation for the relationship between the thinning, the stretched structure, and development of intense current density. Our analysis of this event suggests that (1) the thinning in this event is an MHD force-balanced self-evolving process and is not a forced process due to an increased lobe field; (2) the thinning changes flux tube structure in length and curvature but not significantly in volume; (3) the thinning evolves with a change of the radial plasma pressure profile in the near-Earth tail, which is associated with a locally intensified current sheet. The conclusion is that the increased lobe field strength is not the necessary and the primary cause for cross tail current sheet thinning but rather thinning can occur within the plasma sheet as a result of unknown internal processes.
C1 [Saito, M. H.; Fairfield, D.; Le, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
   [Auster, U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys Tech, D-38106 Braunschweig, Germany.
   [McFadden, J. P.; Bonnell, J. W.; Larson, D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Hau, L. -N.] Natl Cent Univ, Inst Space Sci, Jhongli 32001, Taiwan.
RP Saito, MH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM miho.hasegawa@nasa.gov
RI Le, Guan/C-9524-2012
OI Le, Guan/0000-0002-9504-5214
FU National Science Council of the Republic of China [NSC
   97-2111-M-008-006-MY3]
FX MS thanks L. Chen and C. Z. Cheng for helpful comments and insights. MS
   is also grateful for D. Wolf and J. Yang for important aspects and
   information obtained by the equilibrium version of the Rice Convection
   Model. We thank one of reviewers for pointing out a validity of the MHD
   regime. We acknowledge S. Mende, C. T. Russell, and I. Mann for THEMIS
   GBO/GMAGs, and the CSA for support of the CARISMA network. Solar wind
   data are from NASA OMNIWeb Plus Interface. This research was supported
   in part by an appointment to the NASA Postdoctoral Program at Goddard
   Space Flight Center, administered by Oak Ridge Associated Universities
   through a contract with NASA. This research is supported in part by the
   National Science Council of the Republic of China under grant NSC
   97-2111-M-008-006-MY3 to National Central University.
NR 44
TC 13
Z9 13
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 19
PY 2011
VL 116
AR A10217
DI 10.1029/2011JA016654
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 836ZF
UT WOS:000296158300003
ER

PT J
AU Rummeli, MH
   Rocha, CG
   Ortmann, F
   Ibrahim, I
   Sevincli, H
   Borrnert, F
   Kunstmann, J
   Bachmatiuk, A
   Potschke, M
   Shiraishi, M
   Meyyappan, M
   Buchner, B
   Roche, S
   Cuniberti, G
AF Ruemmeli, Mark H.
   Rocha, Claudia G.
   Ortmann, Frank
   Ibrahim, Imad
   Sevincli, Haldun
   Boerrnert, Felix
   Kunstmann, Jens
   Bachmatiuk, Alicja
   Poetschke, Markus
   Shiraishi, Masashi
   Meyyappan, M.
   Buechner, Bernd
   Roche, Stephan
   Cuniberti, Gianaurelio
TI Graphene: Piecing it Together
SO ADVANCED MATERIALS
LA English
DT Article
ID CHEMICAL-VAPOR-DEPOSITION; FIELD-EFFECT TRANSISTORS; NITROGEN-DOPED
   GRAPHENE; FEW-LAYER GRAPHENE; EPITAXIAL-GRAPHENE; CARBON NANOTUBES;
   LARGE-AREA; ROOM-TEMPERATURE; SILICON-CARBIDE; THIN-FILM
AB Graphene has a multitude of striking properties that make it an exceedingly attractive material for various applications, many of which will emerge over the next decade. However, one of the most promising applications lie in exploiting its peculiar electronic properties which are governed by its electrons obeying a linear dispersion relation. This leads to the observation of half integer quantum hall effect and the absence of localization. The latter is attractive for graphene-based field effect transistors. However, if graphene is to be the material for future electronics, then significant hurdles need to be surmounted, namely, it needs to be mass produced in an economically viable manner and be of high crystalline quality with no or virtually no defects or grains boundaries. Moreover, it will need to be processable with atomic precision. Hence, the future of graphene as a material for electronic based devices will depend heavily on our ability to piece graphene together as a single crystal and define its edges with atomic precision. In this progress report, the properties of graphene that make it so attractive as a material for electronics is introduced to the reader. The focus then centers on current synthesis strategies for graphene and their weaknesses in terms of electronics applications are highlighted.
C1 [Ruemmeli, Mark H.; Ibrahim, Imad; Boerrnert, Felix; Bachmatiuk, Alicja; Buechner, Bernd] Leibniz Inst Festkorper & Werkstoffforsch Dresden, D-01171 Dresden, Germany.
   [Rocha, Claudia G.; Sevincli, Haldun; Kunstmann, Jens; Poetschke, Markus; Cuniberti, Gianaurelio] Tech Univ Dresden, Inst Mat Sci, D-01062 Dresden, Germany.
   [Rocha, Claudia G.; Sevincli, Haldun; Kunstmann, Jens; Poetschke, Markus; Roche, Stephan; Cuniberti, Gianaurelio] Tech Univ Dresden, Max Bergmann Ctr Biomat, D-01062 Dresden, Germany.
   [Ortmann, Frank] CEA Grenoble, INAC SPrAM, F-38054 Grenoble, France.
   [Shiraishi, Masashi] Osaka Univ, Grad Sch Engn Sci, Toyonaka, Osaka 5608531, Japan.
   [Meyyappan, M.; Cuniberti, Gianaurelio] POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea.
   [Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
   [Roche, Stephan] ICN CSIC, CIN2, Bellaterra 08193, Barcelona, Spain.
   [Roche, Stephan] Univ Autonoma Barcelona, Catalan Inst Nanotechnol, Bellaterra 08193, Barcelona, Spain.
   [Roche, Stephan] ICREA, Barcelona 08010, Spain.
RP Rummeli, MH (reprint author), Leibniz Inst Festkorper & Werkstoffforsch Dresden, PF 27 01 16, D-01171 Dresden, Germany.
EM m.ruemmeli@ifw-dresden.de; g.cuniberti@tu-dresden.de
RI Kunstmann, Jens/F-7082-2010; Ortmann, Frank/A-6231-2012; Borrnert,
   Felix/E-8612-2010; Roche, Stephan/B-1116-2012; Poetschke,
   Markus/G-3564-2010; Rummeli, Mark/F-5152-2013; Gomes da Rocha,
   Claudia/B-5673-2011; Shiraishi, Masashi/H-4970-2014; Buchner,
   Bernd/E-2437-2016; Cuniberti, Gianaurelio/B-7192-2008
OI Rummeli, Mark Hermann/0000-0003-3736-6439; Sevincli,
   Haldun/0000-0002-1896-2588; Borrnert, Felix/0000-0002-6892-5320; Roche,
   Stephan/0000-0003-0323-4665; Gomes da Rocha,
   Claudia/0000-0002-2779-9452; Buchner, Bernd/0000-0002-3886-2680;
   Cuniberti, Gianaurelio/0000-0002-6574-7848
FU EU (ECEMP); Freistaat Sachsen; DAAD [A/07/80841]; DFG [RU 1540/8-1];
   Alexander von Humboldt Foundation; BMBF; European Commission; World
   Class University through the National Research Foundation of Korea;
   Ministry of Education, Science and Technology [R31-2008-000-10100-0]
FX MHR thanks the EU (ECEMP) and the Freistaat Sachsen, II the DAAD
   (A/07/80841), FB the DFG (RU 1540/8-1), AB, CGR and SR the Alexander von
   Humboldt Foundation and the BMBF, FO would like to thank the European
   Commission for a Marie Curie Fellowship. MM and GC acknowledge support
   by the World Class University program through the National Research
   Foundation of Korea funded by the Ministry of Education, Science and
   Technology under Project R31-2008-000-10100-0. We are grateful to
   Sandeep M. Gorontla for help in the production of the table of contents
   figure.
NR 269
TC 76
Z9 76
U1 13
U2 183
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 0935-9648
J9 ADV MATER
JI Adv. Mater.
PD OCT 18
PY 2011
VL 23
IS 39
BP 4471
EP 4490
DI 10.1002/adma.201101855
PG 20
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
   Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
   Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
   Physics
GA 847XM
UT WOS:000297008100001
PM 22103000
ER

PT J
AU Samsonov, AA
   Sibeck, DG
   Zolotova, NV
   Biernat, HK
   Chen, SH
   Rastaetter, L
   Singer, HJ
   Baumjohann, W
AF Samsonov, A. A.
   Sibeck, D. G.
   Zolotova, N. V.
   Biernat, H. K.
   Chen, S. -H.
   Rastaetter, L.
   Singer, H. J.
   Baumjohann, W.
TI Propagation of a sudden impulse through the magnetosphere initiating
   magnetospheric Pc5 pulsations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PERIOD MAGNETIC PULSATIONS; FIELD LINE RESONANCES; DAWN-DUSK ASYMMETRY;
   SOLAR-WIND SHOCK; BOW SHOCK; INTERPLANETARY SHOCKS; EARTHS
   MAGNETOSPHERE; DIPOLE MODEL; ALFVEN WAVES; ULF WAVES
AB We compare multipoint observations of an interplanetary shock's interaction with the Earth's magnetosphere on 29 July 2002 with results from global MHD simulations. The sudden impulse associated with the shock's arrival initiates global ultralow-frequency waves with periods from 2 to 5 min. We interpret four cycles of Bz oscillations with T = similar to 3 min at Geotail in the postdawn magnetosphere as radial magnetopause oscillations. GOES 8, in the same late morning sector, observed compressional and toroidal waves with the same frequency at the same time. GOES 10, in the early morning sector, observed toroidal waves with a slightly lower period. We suggest that these observations confirm the mode coupling theory. The interplanetary shock initiates compressional magnetospheric waves which, according to our estimates, oscillate between the ionosphere and magnetopause and gradually convert their energy into that of standing Alfven waves. At the same time, Polar in the outer predawn magnetosphere observed strong velocity oscillations and weak magnetic field oscillations with a similar to 4 min period. Global MHD models successfully predict these oscillations and connect them to the Kelvin-Helmholtz instability which results in large flow vortices with sizes of about ten Earth radii. However, the global models do not predict the multiple compressional oscillations with the observed periods and therefore cannot readily explain the GOES observations.
C1 [Samsonov, A. A.; Biernat, H. K.; Baumjohann, W.] Space Res Inst, A-8042 Graz, Austria.
   [Samsonov, A. A.; Zolotova, N. V.] St Petersburg State Univ, Dept Earth Phys, St Petersburg 198504, Russia.
   [Sibeck, D. G.; Chen, S. -H.; Rastaetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Singer, H. J.] NOAA, Space Weather Predict Ctr, Boulder, CO 80305 USA.
RP Samsonov, AA (reprint author), Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria.
EM andre.samsonov@gmail.com; david.g.sibeck@nasa.gov; ned@geo.phys.spbu.ru;
   helfried.biernat@oeaw.ac.at; sheng-hsien.chen@nasa.gov;
   lutz.rastaetter-1@nasa.gov; howard.singer@noaa.gov;
   baumjohann@oeaw.ac.at
RI Sibeck, David/D-4424-2012; Rastaetter, Lutz/D-4715-2012; Baumjohann,
   Wolfgang/A-1012-2010; Samsonov, Andrey/I-7057-2012; Zolotova,
   Nadezhda/I-7061-2012
OI Rastaetter, Lutz/0000-0002-7343-4147; Baumjohann,
   Wolfgang/0000-0001-6271-0110; Samsonov, Andrey/0000-0001-8243-1151;
   Zolotova, Nadezhda/0000-0002-0019-2415
FU NASA
FX This work was supported by NASA's Guest Investigator program. A.A.S.
   thanks Andriy Koval for providing the code for shock normal calculations
   and Prof. Victor Sergeev for valuable comments. We thank Ruth Skoug for
   explanations about ACE SWEPAM measurements. This research made use of
   Geotail data obtained from Data Archives and Transmission System
   (DARTS), provided by Center for Science-satellite Operation and Data
   Archives (C-SODA) at ISAS/JAXA. ACE data were provided by the ACE/MAG
   and ACE/SWEPAM instrument teams at the ACE Science Center
   (http://www.srl.caltech.edu/ACE/). LANL digital moments were provided by
   the MPA team through the Coordinated Data Analysis Web
   (http://cdaweb.gsfc.nasa.gov). Simulation results have been provided by
   the Community Coordinated Modeling Center (http://ccmc.gsfc.nasa.gov) at
   Goddard Space Flight Center. The LFM-MIX model was developed at the
   Center for Integrated Space Weather Modeling (CISM), the OpenGGCM was
   developed at the University of New Hampshire, and the SWMF was developed
   at the University of Michigan. We have studied the runs
   Andrey_Samsonov_082310_2, Andrey_Samsonov_101510_1,
   Andrey_Samsonov_020811_1, Andrey_Samsonov_021011_1, and
   Andrey_Samsonov022211_1.
NR 59
TC 16
Z9 16
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 18
PY 2011
VL 116
AR A10216
DI 10.1029/2011JA016706
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 836ZB
UT WOS:000296157800006
ER

PT J
AU Anschutz, H
   Sinisalo, A
   Isaksson, E
   McConnell, JR
   Hamran, SE
   Bisiaux, MM
   Pasteris, D
   Neumann, TA
   Winther, JG
AF Anschutz, H.
   Sinisalo, A.
   Isaksson, E.
   McConnell, J. R.
   Hamran, S. -E.
   Bisiaux, M. M.
   Pasteris, D.
   Neumann, T. A.
   Winther, J. -G.
TI Variation of accumulation rates over the last eight centuries on the
   East Antarctic Plateau derived from volcanic signals in ice cores
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DRONNING MAUD-LAND; SURFACE MASS-BALANCE; SHALLOW FIRN CORES; SEA-LEVEL
   RISE; SNOW ACCUMULATION; VARIABILITY; RECORD; SHEET; DOME; AMUNDSENISEN
AB Volcanic signatures in ice-core records provide an excellent means to date the cores and obtain information about accumulation rates. From several ice cores it is thus possible to extract a spatio-temporal accumulation pattern. We show records of electrical conductivity and sulfur from 13 firn cores from the Norwegian-USA scientific traverse during the International Polar Year 2007-2009 (IPY) through East Antarctica. Major volcanic eruptions are identified and used to assess century-scale accumulation changes. The largest changes seem to occur in the most recent decades with accumulation over the period 1963-2007/08 being up to 25% different from the long-term record. There is no clear overall trend, some sites show an increase in accumulation over the period 1963 to present while others show a decrease. Almost all of the sites above 3200 m above sea level (asl) suggest a decrease. These sites also show a significantly lower accumulation value than large-scale assessments both for the period 1963 to present and for the long-term mean at the respective drill sites. The spatial accumulation distribution is influenced mainly by elevation and distance to the ocean (continentality), as expected. Ground-penetrating radar data around the drill sites show a spatial variability within 10-20% over several tens of kilometers, indicating that our drill sites are well representative for the area around them. Our results are important for large-scale assessments of Antarctic mass balance and model validation.
C1 [Anschutz, H.; Isaksson, E.; Winther, J. -G.] Norwegian Polar Res Inst, Fram Ctr, N-9296 Tromso, Norway.
   [Sinisalo, A.; Hamran, S. -E.] Univ Oslo, Dept Geosci, N-0316 Oslo, Norway.
   [McConnell, J. R.; Bisiaux, M. M.; Pasteris, D.] Desert Res Inst, Div Hydrol Sci, Reno, NV 89512 USA.
   [Hamran, S. -E.] Forsvarets Forskningsinst, Lillestrom, Norway.
   [Neumann, T. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Anschutz, H (reprint author), Norwegian Geotech Inst, Div Geomat Integrated Geosci, Oslo, Norway.
EM helgard.anschuetz@npolar.no
RI Neumann, Thomas/D-5264-2012
FU Norwegian Polar Institute [152]; Research Council of Norway; National
   Science Foundation of the USA
FX This work has been carried out under the umbrella of TASTE-IDEA within
   the framework of IPY project 152 funded by Norwegian Polar Institute,
   the Research Council of Norway and the National Science Foundation of
   the USA. This work is also a contribution to ITASE. The help of several
   people in the lab is gratefully acknowledged. Special thanks go to the
   traverse teams. K. Langley and S. Tronstad (Norwegian Polar Institute)
   helped with Figure 1. Thoughtful comments by three reviewers helped to
   improve the manuscript.
NR 46
TC 14
Z9 14
U1 1
U2 16
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 OCT 18
PY 2011
VL 116
AR D20103
DI 10.1029/2011JD015753
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 836ZN
UT WOS:000296159800004
ER

PT J
AU Kahn, BH
   Nasiri, SL
   Schreier, MM
   Baum, BA
AF Kahn, Brian H.
   Nasiri, Shaima L.
   Schreier, Mathias M.
   Baum, Bryan A.
TI Impacts of subpixel cloud heterogeneity on infrared thermodynamic phase
   assessment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RESOLUTION IMAGING SPECTRORADIOMETER; GENERAL-CIRCULATION MODEL;
   CARBON-DIOXIDE; PART I; RADIATIVE-TRANSFER; WATER-VAPOR; THIN CIRRUS;
   MODIS; CLIMATE; SOUNDER
AB A combination of spatially collocated Atmospheric Infrared Sounder (AIRS) radiances and Moderate Resolution Imaging Spectroradiometer (MODIS) cloud products are used to quantify the impact of cloud heterogeneity on AIRS-based assessments of cloud thermodynamic phase. While radiative transfer simulations have demonstrated that selected AIRS channels have greater sensitivity to cloud thermodynamic phase in comparison to the relevant MODIS bands, the relative trade-offs of spectral and spatial resolution differences that are inherent between AIRS and MODIS have not been quantified. Global distributions of AIRS field-of-view scale frequencies of clear sky (13-14%), heterogeneous cloud (26-28%), and homogeneous cloud (59-60%) are quantified for a four week time period using cloud fraction, and further categorization of cloud uniformity is assessed with the variance of cloud top temperature. Homogeneous clouds with window brightness temperatures (T-b) between 250 and 265 K are shown to have larger cloud thermodynamic phase signatures than heterogeneous clouds. Clouds in this limited T-b range occur 30-50% of the time in the mid-and high latitude storm track regions, are generally difficult to identify as being water or ice phase, and show strong responses in forced CO2 climate change modeling experiments. Two-dimensional histograms of T-b differences sensitive to cloud phase (1231-960 cm(-1)) and column water vapor (1231-1227 cm(-1)) show distinct differences between many homogeneous and heterogeneous cloud scenes. The results suggest the potential for a quantitative approach using a combination of hyperspectral sounders with high-spatial-resolution imagers, and their derived geophysical products, to assess cloud thermodynamic phase estimates within increasingly complex subpixel-scale cloud variability.
C1 [Kahn, Brian H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Nasiri, Shaima L.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
   [Schreier, Mathias M.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
   [Baum, Bryan A.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
RP Kahn, BH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-237, Pasadena, CA 91109 USA.
EM brian.h.kahn@jpl.nasa.gov
RI Nasiri, Shaima/C-8044-2011; Baum, Bryan/B-7670-2011
OI Baum, Bryan/0000-0002-7193-2767
FU NASA [NNX08AI09G]; AIRS at the Jet Propulsion Laboratory (JPL)
FX The authors gratefully acknowledge the constructive feedback of the
   anonymous reviewers. Funding for BHK and MMS was provided in part by
   NASA award NNX08AI09G and the AIRS project at the Jet Propulsion
   Laboratory (JPL). AIRS and MODIS data were obtained through the Goddard
   Earth Sciences Data and Information Services Center
   (http://daac.gsfc.nasa.gov). A portion of this work was performed within
   the Joint Institute for Regional Earth System Science and Engineering
   (JIFRESSE) of the University of California, Los Angeles (UCLA) and at
   the Jet Propulsion Laboratory, California Institute of Technology, under
   contract with NASA. (C) 2011 California Institute of Technology.
   Government sponsorship is acknowledged.
NR 61
TC 6
Z9 6
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 18
PY 2011
VL 116
AR D20201
DI 10.1029/2011JD015774
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 836ZN
UT WOS:000296159800005
ER

PT J
AU Veraverbeke, S
   Harris, S
   Hook, S
AF Veraverbeke, S.
   Harris, S.
   Hook, S.
TI Evaluating spectral indices for burned area discrimination using
   MODIS/ASTER (MASTER) airborne simulator data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Fire; Burned area mapping; Southern California; Emissivity; Moderate
   Resolution Imaging Spectroradiometer; Advanced Spaceborne and Thermal
   Emission Radiometer; Normalized Burn Ratio
ID ADJUSTED VEGETATION INDEX; NORTHERN BAJA-CALIFORNIA; LANDSAT-TM;
   SOUTHERN-CALIFORNIA; FIRE SEVERITY; SPOT-VEGETATION; BOREAL FOREST;
   TIME-SERIES; IMAGERY; MODIS
AB Wildland fires are an annually recurring phenomenon in many terrestrial ecosystems. Accurate burned area estimates are important for modeling fire-induced trace gas emissions and rehabilitating post-fire landscapes. High spatial and spectral resolution MODIS/ASTER (MASTER) airborne simulator data acquired over three 2007 southern California burns were used to evaluate the sensitivity of different spectral indices at discriminating burned land shortly after a fire. The performance of the indices, which included both traditional and new band combinations, was assessed by means of a separability index that provides an assessment of the effectiveness of a given index at discriminating between burned and unburned land. In the context of burned land applications results demonstrated (i) that the highest sensitivity of the longer short wave infrared (SWIR) spectral region (1.9 to 2.5 mu m) was found at the band interval from 2.31 to 2.36 mu m, (ii) the high discriminatory power of the mid infrared spectral domain (3 to 5.5 mu m) and (iii) the high potential of emissivity data. As a consequence, a newly proposed index which combined near infrared (NIR), longer SWIR and emissivity outperformed all other indices when results were averaged over the three fires. Results were slightly different between land cover types (shrubland vs. forest-woodland). Prior to use in the indices the thermal infrared data were separated into temperature and emissivity to assess the benefits of using both temperature and emissivity. Currently, the only spaceborne sensor that provides moderate spatial resolution (<100 m) temperature and emissivity data is the Advanced Spaceborne and Thermal Emission Radiometer (ASTER). Therefore, our findings can open new perspectives for the utility of future sensors, such as the Hyperspectral Infrared (HyspIRI) sensor. However, further research is required to evaluate the performance of the newly proposed band combinations in other vegetation types and different fire regimes. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Veraverbeke, S.; Harris, S.; Hook, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Harris, S.] Monash Univ, Sch Geog & Environm Sci, Melbourne, Vic 3800, Australia.
RP Veraverbeke, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sander.S.Veraverbeke@jpl.nasa.gov; sarah.harris@monash.edu;
   Simon.J.Hook@jpl.nasa.gov
RI Veraverbeke, Sander/H-2301-2012
OI Veraverbeke, Sander/0000-0003-1362-5125
NR 79
TC 23
Z9 27
U1 3
U2 19
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 OCT 17
PY 2011
VL 115
IS 10
BP 2702
EP 2709
DI 10.1016/j.rse.2011.06.010
PG 8
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
   Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
   Photographic Technology
GA 809EF
UT WOS:000294033900023
ER

PT J
AU Wang, Y
   Czapla-Myers, J
   Lyapustin, A
   Thome, K
   Dutton, EG
AF Wang, Y.
   Czapla-Myers, J.
   Lyapustin, A.
   Thome, K.
   Dutton, E. G.
TI AERONET-based surface reflectance validation network (ASRVN) data
   evaluation: Case study for railroad valley calibration site
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE AERONET-based Surface Reflectance; Validation Network; Atmospheric
   Correction; BRF; HDRF; Surface Reflectance; Surface Albedo; AERONET;
   Validation; MODIS
ID MODIS-LAI PRODUCT; VICARIOUS CALIBRATION; MULTISCALE ANALYSIS; ALBEDO;
   ALGORITHM; BRDF
AB The AERONET-based Surface Reflectance Validation Network (ASRVN) is an operational processing system developed for validation of satellite derived surface reflectance products at regional and global scales. The ASRVN receives 50 x 50 km(2) subsets of MODIS data centered at AERONET sites along with AERONET aerosol and water vapor data, and performs an atmospheric correction. The ASRVN produces surface bidirectional reflectance factor (BRF), albedo, parameters of the Ross-Thick Li-Sparse (RTLS) BRF model, as well as Hemispherical-Directional Reflectance Factor (HDRF), which is required for comparison with the ground-based measurements. This paper presents a comparison of ASRVN HDRF with the ground-based HDRF measurements collected during 2001-2008 over a bright calibration Railroad Valley, Nevada site as part of the MODIS land validation program. The ground measurements were conducted by the Remote Sensing Group (RSG) at the University of Arizona using an ASD spectrometer. The study reveals a good agreement between ASRVN and RSG HDRF for both MODIS Terra and Aqua with rmse -0.01-0.025 in the 500 m MODIS land bands B1-B7. Obtained rinse is below uncertainties due to the spatial and seasonal variability of the bright calibration 1 km(2) area. While two MODIS instruments have a similar rmse in the visible bands, MODIS Aqua has a better agreement (lower arise) with the ground data than MODIS Terra at wavelengths 0.87-2.1 mu m. An independent overall good agreement of two MODIS instruments with the ground data indicates that the relative calibration of MODIS Terra and Aqua at medium-to-bright reflectance levels for the stated time period is significantly better than uncertainties of the ASRVN and ground data. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Wang, Y.; Lyapustin, A.; Thome, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Wang, Y.] Univ Maryland Baltimore Cty, GEST Ctr, Catonsville, MD 21228 USA.
   [Czapla-Myers, J.] Univ Arizona, Ctr Opt Sci, Remote Sensing Grp, Tucson, AZ USA.
   [Dutton, E. G.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
RP Wang, Y (reprint author), NASA, Goddard Space Flight Ctr, Code 614-4, Greenbelt, MD 20771 USA.
EM yujie.wang@nasa.gov
RI Thome, Kurtis/D-7251-2012; Lyapustin, Alexei/H-9924-2014; 
OI Lyapustin, Alexei/0000-0003-1105-5739; Czapla-Myers,
   Jeffrey/0000-0003-4804-5358
NR 29
TC 7
Z9 7
U1 0
U2 10
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 OCT 17
PY 2011
VL 115
IS 10
BP 2710
EP 2717
DI 10.1016/j.rse.2011.06.011
PG 8
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
   Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
   Photographic Technology
GA 809EF
UT WOS:000294033900024
ER

PT J
AU Lawson, JW
   Daw, MS
   Bauschlicher, CW
AF Lawson, John W.
   Daw, Murray S.
   Bauschlicher, Charles W., Jr.
TI Lattice thermal conductivity of ultra high temperature ceramics ZrB2 and
   HfB2 from atomistic simulations
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID MOLECULAR-DYNAMICS SIMULATIONS; ZIRCONIUM DIBORIDE; HAFNIUM DIBORIDE
AB Atomistic Green-Kubo simulations are performed to evaluate the lattice thermal conductivity for single crystals of the ultra high temperature ceramics ZrB2 and HfB2. Recently developed interatomic potentials are used for these simulations. Heat current correlation functions show rapid oscillations, which can be identified with mixed metal-Boron optical phonon modes. Results for temperatures from 300K to 1000K are presented. (C) 2011 American Institute of Physics. [doi:10.1063/1.3647754]
C1 [Lawson, John W.] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
   [Daw, Murray S.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29631 USA.
   [Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA.
RP Lawson, JW (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, Mail Stop 234-1, Moffett Field, CA 94035 USA.
EM John.W.Lawson@nasa.gov
FU NASA
FX J.W.L. and C. W. B. are civil servants in the Entry Systems and
   Technology Division. M. S. D was supported under a NASA prime contract
   to ELORET Corporation. We benefited from discussions with Pawel
   Keblinski and Tapan Desai.
NR 21
TC 6
Z9 6
U1 4
U2 39
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 OCT 15
PY 2011
VL 110
IS 8
AR 083507
DI 10.1063/1.3647754
PG 4
WC Physics, Applied
SC Physics
GA 841NU
UT WOS:000296519900039
ER

PT J
AU Robertson, FR
   Bosilovich, MG
   Chen, JY
   Miller, TL
AF Robertson, Franklin R.
   Bosilovich, Michael G.
   Chen, Junye
   Miller, Timothy L.
TI The Effect of Satellite Observing System Changes on MERRA Water and
   Energy Fluxes
SO JOURNAL OF CLIMATE
LA English
DT Article
ID 20TH-CENTURY CLIMATE VARIATIONS; NINO-SOUTHERN OSCILLATION; EL-NINO;
   EXTRATROPICAL CIRCULATION; SPATIOTEMPORAL STRUCTURE; ATMOSPHERIC
   CIRCULATION; REDUNDANCY ANALYSIS; DATA ASSIMILATION; ANNULAR MODES; PART
   II
AB Like all reanalysis efforts, the Modern Era Retrospective-Analysis for Research and Applications (MERRA) must contend with an inhomogeneous observing network. Here the effects of the two most obvious observing system epoch changes, the Advanced Microwave Sounding Unit-A (AMSU-A) series in late 1998 and, to a lesser extent, the earlier advent of the Special Sensor Microwave Imager (SSM/I) in late 1987 are examined. These sensor changes affect model moisture and enthalpy increments and thus water and energy fluxes, since the latter result from model physics processes that respond sensitively to state variable forcing. Inclusion of the analysis increments in the MERRA dataset is a unique feature among reanalyses that facilitates understanding the relationships between analysis forcing and flux response.
   In stepwise fashion in time, the vertically integrated global-mean moisture increments change sign from drying to moistening and heating increments drop nearly 15 W m(-2) over the 30 plus years of the assimilated products. Regression of flux quantities on an El Nino-Southern Oscillation sea surface temperature (SST) index analysis reveals that this mode of climate variability dominates interannual signals and its leading expression is minimally affected by satellite observing system changes. Conversely, precipitation patterns and other fluxes influenced by SST changes associated with Pacific decadal variability (PDV) are significantly distorted. Observing system changes also induce a nonstationary component to the annual cycle signals.
   Principal component regression is found useful for identifying artifacts produced by changes of satellite sensors and defining appropriate adjustments. After the adjustments are applied, the spurious flux trend components are greatly diminished. Time series of the adjusted precipitation and the Global Precipitation Climatology Project (GPCP) data compare favorably on a global basis. The adjustments also provide a much better depiction of precipitation spatial trends associated with PDV-like forcing. The utility as well as associated drawbacks of this statistical adjustment and the prospects for future improvements of the methodology are discussed.
C1 [Robertson, Franklin R.] NASA, Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA.
   [Bosilovich, Michael G.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA.
   [Chen, Junye] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Robertson, FR (reprint author), NASA, Marshall Space Flight Ctr, Earth Sci Off, VP61,320 Sparkman Dr, Huntsville, AL 35805 USA.
EM pete.robertson@nasa.gov
RI Bosilovich, Michael/F-8175-2012
FU NASA Energy and Water Cycle Study (NEWS); NASA Modeling, Analysis, and
   Prediction (MAP)
FX This study was supported by the NASA Energy and Water Cycle Study (NEWS)
   and by the NASA Modeling, Analysis, and Prediction (MAP) Program. The
   authors thank Dr. Emily Liu, GSFC, for producing the MERRA withholding
   experiments and for discussions of these results. Also, Drs. Max Suarez
   and Siegfried Schubert provided many thoughtful comments and discussions
   concerning the results in this paper. We are especially grateful to Dr.
   Ron Gelaro, whose comments substantially improved an earlier version of
   this paper.
NR 45
TC 46
Z9 48
U1 1
U2 6
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 OCT 15
PY 2011
VL 24
IS 20
BP 5197
EP 5217
DI 10.1175/2011JCLI4227.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 840XZ
UT WOS:000296476700001
ER

PT J
AU Teixeira, J
   Cardoso, S
   Bonazzola, M
   Cole, J
   DelGenio, A
   DeMott, C
   Franklin, C
   Hannay, C
   Jakob, C
   Jiao, Y
   Karlsson, J
   Kitagawa, H
   Kohler, M
   Kuwano-Yoshida, A
   LeDrian, C
   Li, J
   Lock, A
   Miller, MJ
   Marquet, P
   Martins, J
   Mechoso, CR
   Meijgaard, EV
   Meinke, I
   Miranda, PMA
   Mironov, D
   Neggers, R
   Pan, HL
   Randall, DA
   Rasch, PJ
   Rockel, B
   Rossow, WB
   Ritter, B
   Siebesma, AP
   Soares, PMM
   Turk, FJ
   Vaillancourt, PA
   Von Engeln, A
   Zhao, M
AF Teixeira, J.
   Cardoso, S.
   Bonazzola, M.
   Cole, J.
   DelGenio, A.
   DeMott, C.
   Franklin, C.
   Hannay, C.
   Jakob, C.
   Jiao, Y.
   Karlsson, J.
   Kitagawa, H.
   Koehler, M.
   Kuwano-Yoshida, A.
   LeDrian, C.
   Li, J.
   Lock, A.
   Miller, M. J.
   Marquet, P.
   Martins, J.
   Mechoso, C. R.
   Meijgaard, E. V.
   Meinke, I.
   Miranda, P. M. A.
   Mironov, D.
   Neggers, R.
   Pan, H. L.
   Randall, D. A.
   Rasch, P. J.
   Rockel, B.
   Rossow, W. B.
   Ritter, B.
   Siebesma, A. P.
   Soares, P. M. M.
   Turk, F. J.
   Vaillancourt, P. A.
   Von Engeln, A.
   Zhao, M.
TI Tropical and Subtropical Cloud Transitions in Weather and Climate
   Prediction Models: The GCSS/WGNE Pacific Cross-Section Intercomparison
   (GPCI)
SO JOURNAL OF CLIMATE
LA English
DT Article
ID GENERAL-CIRCULATION MODELS; SHALLOW CUMULUS CONVECTION; BOUNDARY-LAYER
   CLOUDS; RADIATION BUDGET EXPERIMENT; COMMUNITY ATMOSPHERE MODEL;
   LARGE-SCALE MODELS; PART I; TOGA-COARE; ECMWF REANALYSIS; RESOLVING
   MODEL
AB A model evaluation approach is proposed in which weather and climate prediction models are analyzed along a Pacific Ocean cross section, from the stratocumulus regions off the coast of California, across the shallow convection dominated trade winds, to the deep convection regions of the ITCZ-the Global Energy and Water Cycle Experiment Cloud System Study/Working Group on Numerical Experimentation (GCSS/WGNE) Pacific Cross-Section Intercomparison (GPCI). The main goal of GPCI is to evaluate and help understand and improve the representation of tropical and subtropical cloud processes in weather and climate prediction models. In this paper, a detailed analysis of cloud regime transitions along the cross section from the subtropics to the tropics for the season June-July-August of 1998 is presented. This GPCI study confirms many of the typical weather and climate prediction model problems in the representation of clouds: underestimation of clouds in the stratocumulus regime by most models with the corresponding consequences in terms of shortwave radiation biases; overestimation of clouds by the 40-yr ECMWF Re-Analysis (ERA-40) in the deep tropics (in particular) with the corresponding impact in the outgoing longwave radiation; large spread between the different models in terms of cloud cover, liquid water path and shortwave radiation; significant differences between the models in terms of vertical cross sections of cloud properties (in particular), vertical velocity, and relative humidity. An alternative analysis of cloud cover mean statistics is proposed where sharp gradients in cloud cover along the GPCI transect are taken into account. This analysis shows that the negative cloud bias of some models and ERA-40 in the stratocumulus regions [as compared to the first International Satellite Cloud Climatology Project (ISCCP)] is associated not only with lower values of cloud cover in these regimes, but also with a stratocumulus-to-cumulus transition that occurs too early along the trade wind Lagrangian trajectory. Histograms of cloud cover along the cross section differ significantly between models. Some models exhibit a quasi-bimodal structure with cloud cover being either very large (close to 100%) or very small, while other models show a more continuous transition. The ISCCP observations suggest that reality is in-between these two extreme examples. These different patterns reflect the diverse nature of the cloud, boundary layer, and convection parameterizations in the participating weather and climate prediction models.
C1 [Teixeira, J.; Li, J.; Turk, F. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Cardoso, S.; Martins, J.; Miranda, P. M. A.; Soares, P. M. M.] Univ Lisbon, Inst Dom Luis, P-1699 Lisbon, Portugal.
   [Cardoso, S.; Hannay, C.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
   [Bonazzola, M.] Meteorol Dynam Lab, Paris, France.
   [Cole, J.] Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada.
   [DelGenio, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [DeMott, C.; Randall, D. A.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
   [Franklin, C.] Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia.
   [Jakob, C.] Monash Univ, Melbourne, Vic 3004, Australia.
   [Jiao, Y.] Univ Quebec, Dept Earth & Atmospher Sci, Montreal, PQ H3C 3P8, Canada.
   [Karlsson, J.] Stockholm Univ, S-10691 Stockholm, Sweden.
   [Kitagawa, H.] Japan Meteorol Agcy, Tokyo, Japan.
   [Koehler, M.; Miller, M. J.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
   [Kuwano-Yoshida, A.] Japan Agcy Marine Earth Sci & Technol, Earth Simulator Ctr, Computat Earth Sci Res Program, Yokohama, Kanagawa, Japan.
   [LeDrian, C.] Eidgenoss Tech Hsch Zentrum, Inst Atmospher & Climate Sci, Zurich, Switzerland.
   [Lock, A.] United Kingdom Meteorol Off, Exeter, Devon, England.
   [Marquet, P.] Ctr Natl Rech Meteorol, Toulouse, France.
   [Mechoso, C. R.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
   [Meijgaard, E. V.; Neggers, R.; Siebesma, A. P.] Koninklijk Nederlands Meteorol Inst, De Bilt, Netherlands.
   [Meinke, I.] Univ Calif San Diego, Expt Climate Predict Ctr, La Jolla, CA 92093 USA.
   [Mironov, D.; Ritter, B.] Deutsch Wetterdienst, Div Res & Dev, Offenbach, Germany.
   [Pan, H. L.] Natl Ctr Environm Predict, Environm Modeling Ctr, Camp Springs, MD USA.
   [Rasch, P. J.] Pacific NW Natl Lab, Richland, WA 99352 USA.
   [Rockel, B.] GKSS Forschungszentrum Geesthacht GmbH, Inst Coastal Res, Geesthacht, Germany.
   [Rossow, W. B.] CUNY City Coll, CREST, New York, NY 10031 USA.
   [Vaillancourt, P. A.] Environm Canada, Canadian Meteorol Ctr, Rech Previs Numer, Dorval, PQ, Canada.
   [Von Engeln, A.] EUMETSAT, Darmstadt, Germany.
   [Zhao, M.] Geophys Fluid Dynam Lab, Princeton, NJ USA.
RP Teixeira, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM joao.teixeira@jpl.nasa.gov
RI Randall, David/E-6113-2011; Miranda, Pedro/B-6971-2008; Karlsson,
   Johannes/H-3937-2011; Jakob, Christian/A-1082-2010; Franklin,
   Charmaine/C-9278-2012; Del Genio, Anthony/D-4663-2012; Soares, Pedro
   /K-6239-2012; Zhao, Ming/C-6928-2014; Kuwano-Yoshida, Akira/I-8652-2014;
   Rossow, William/F-3138-2015; Martins, Joao/C-1713-2009; DeMott,
   Charlotte/L-7414-2015
OI Randall, David/0000-0001-6935-4112; Miranda, Pedro/0000-0002-4288-9456;
   Jakob, Christian/0000-0002-5012-3207; Del Genio,
   Anthony/0000-0001-7450-1359; Soares, Pedro /0000-0002-9155-5874;
   Kuwano-Yoshida, Akira/0000-0003-3151-8550; Martins,
   Joao/0000-0003-4117-0754; DeMott, Charlotte/0000-0002-3975-1288
FU NASA; Office of Naval Research
FX We acknowledge the crucial feedback received from a variety of
   participants in the workshops and conferences where results of this
   study have been presented and discussed. JT and SC acknowledge the
   support of the NASA MAP program and the Office of Naval Research. Part
   of the research described in this publication was carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration. We
   acknowledge the important feedback from the four anonymous referees.
NR 97
TC 53
Z9 53
U1 2
U2 21
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD OCT 15
PY 2011
VL 24
IS 20
BP 5223
EP 5256
DI 10.1175/2011JCLI3672.1
PG 34
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 840XZ
UT WOS:000296476700003
ER

PT J
AU Qian, LY
   Burns, AG
   Chamberlin, PC
   Solomon, SC
AF Qian, Liying
   Burns, Alan G.
   Chamberlin, Phillip C.
   Solomon, Stanley C.
TI Variability of thermosphere and ionosphere responses to solar flares
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; EXTREME ULTRAVIOLET EMISSION; TOTAL
   ELECTRON-CONTENT; LATENT-HEAT RELEASE; MASS-SPECTROMETER;
   EMPIRICAL-MODEL; ATMOSPHERE; MISSION; ELECTRODYNAMICS; TIDES
AB We investigated how the rise rate and decay rate of solar flares affect the thermosphere and ionosphere responses to them. Model simulations and data analysis were conducted for two flares of similar magnitude (X6.2 and X5.4) that had the same location on the solar limb, but the X6.2 flare had longer rise and decay times. Simulated total electron content (TEC) enhancements from the X6.2 and X5.4 flares were similar to 6 total electron content units (TECU) and similar to 2 TECU, and the simulated neutral density enhancements were similar to 15%-20% and similar to 5%, respectively, in reasonable agreement with observations. Additional model simulations showed that for idealized flares with the same magnitude and location, the thermosphere and ionosphere responses changed significantly as a function of rise and decay rates. The "Neupert Effect," which predicts that a faster flare rise rate leads to a larger EUV enhancement during the impulsive phase, caused a larger maximum ion production enhancement. In addition, model simulations showed that increased E x B plasma transport due to conductivity increases during the flares caused a significant equatorial anomaly feature in the electron density enhancement in the F region but a relatively weaker equatorial anomaly feature in TEC enhancement, owing to dominant contributions by photochemical production and loss processes. The latitude dependence of the thermosphere response correlated well with the solar zenith angle effect, whereas the latitude dependence of the ionosphere response was more complex, owing to plasma transport and the winter anomaly.
C1 [Qian, Liying; Burns, Alan G.; Solomon, Stanley C.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
   [Chamberlin, Phillip C.] NASA, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Qian, LY (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA.
EM lqian@ucar.edu
RI Chamberlin, Phillip/C-9531-2012; Solomon, Stanley/J-4847-2012; Qian,
   Liying/D-9236-2013; Burns, Alan/L-1547-2013
OI Chamberlin, Phillip/0000-0003-4372-7405; Solomon,
   Stanley/0000-0002-5291-3034; Qian, Liying/0000-0003-2430-1388; 
FU NASA [NNX08AQ31G, NNX09AJ60G]; National Science Foundation
FX This research was supported by NASA grants NNX08AQ31G and NNX09AJ60G to
   the National Center for Atmospheric Research. NCAR is supported by the
   National Science Foundation.
NR 36
TC 13
Z9 13
U1 1
U2 7
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 OCT 15
PY 2011
VL 116
AR A10309
DI 10.1029/2011JA016777
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 834TP
UT WOS:000295987300006
ER

PT J
AU Heck, PR
   Huberty, JM
   Kita, NT
   Ushikubo, T
   Kozdon, R
   Valley, JW
AF Heck, Philipp R.
   Huberty, Jason M.
   Kita, Noriko T.
   Ushikubo, Takayuki
   Kozdon, Reinhard
   Valley, John W.
TI SIMS analyses of silicon and oxygen isotope ratios for quartz from
   Archean and Paleoproterozoic banded iron formations
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID NUVVUAGITTUQ SUPRACRUSTAL BELT; SOUTH-AFRICA; TRANSVAAL SUPERGROUP;
   WESTERN-AUSTRALIA; FE ISOTOPE; FORMATION DEPOSITION; ATMOSPHERIC OXYGEN;
   STABLE-ISOTOPES; HAMERSLEY GROUP; RICE PLANTS
AB Banded iron formations (BIFs) are chemical marine sediments dominantly composed of alternating iron-rich (oxide, carbonate, sulfide) and silicon-rich (chert, jasper) layers. Isotope ratios of iron, carbon, and sulfur in BIF iron-bearing minerals are biosignatures that reflect microbial cycling for these elements in BIFs. While much attention has focused on iron, banded iron formations are equally banded silica formations. Thus, silicon isotope ratios for quartz can provide insight on the sources and cycling of silicon in BIFs. BIFs are banded by definition, and microlaminae, or sub-mm banding, are characteristic of many BIFs. In situ microanalysis including secondary ion mass spectrometry is well-suited for analyzing such small features. In this study we used a CAMECA IMS-1280 ion microprobe to obtain highly accurate (perpendicular to 0.3 parts per thousand) and spatially resolved (similar to 10 mu m spot size) analyses of silicon and oxygen isotope ratios for quartz from several well known BIFs: Isua, southwest Greenland (similar to 3.8 Ga); Hamersley Group, Western Australia (similar to 2.5 Ga); Transvaal Group, South Africa (similar to 2.5 Ga); and Biwabik Iron Formation, Minnesota, USA (similar to 1.9 Ga). Values of delta(18)O range from +7.9 parts per thousand to +27.5 parts per thousand and include the highest reported delta(18)O values for BIF quartz. Values of delta(30)Si have a range of similar to 5 parts per thousand from -3.7 parts per thousand to +1.2 parts per thousand and extend to the lowest delta(30)Si values for Precambrian cherts. Isua BIF samples are homogeneous in delta(18)O to +/- 0.3 parts per thousand at mm-to cm-scale, but are heterogeneous in delta(30)Si up to 3 parts per thousand, similar to the range in delta(30)Si found in BIFs that have not experienced high temperature metamorphism (up to 300 degrees C). Values of delta(30)Si for quartz are homogeneous to +/- 0.3 parts per thousand in individual sub-mm laminae, but vary by up to 3 parts per thousand between multiple laminae over mm-to-cm of vertical banding. The scale of exchange for Si in quartz in BIFs is thus limited to the size of microlaminae, or less than similar to 1 mm. We interpret differences in delta(30)Si between microlaminae as preserved from primary deposition. Silicon in BIF quartz is mostly of marine hydrothermal origin (delta(30)Si < -0.5 parts per thousand) but silicon from continental weathering (delta(30)Si similar to 1 parts per thousand) was an important source as early as 3.8 Ga. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Heck, Philipp R.; Huberty, Jason M.; Kita, Noriko T.; Ushikubo, Takayuki; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA.
   [Heck, Philipp R.; Huberty, Jason M.; Kita, Noriko T.; Ushikubo, Takayuki; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, WiscSIMS, Dept Geosci, Madison, WI 53706 USA.
   [Heck, Philipp R.] Field Museum, Dept Geol, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
   [Heck, Philipp R.] Univ Chicago, Chicago Ctr Cosmochem, Chicago, IL 60637 USA.
RP Heck, PR (reprint author), Field Museum, Dept Geol, Robert A Pritzker Ctr Meteorit & Polar Studies, 1400 S Lake Shore Dr, Chicago, IL 60605 USA.
EM prheck@fieldmuseum.org
RI Heck, Philipp/C-6092-2012; Kozdon, Reinhard/J-9468-2014; Kita,
   Noriko/H-8035-2016; Valley, John/B-3466-2011
OI Kozdon, Reinhard/0000-0001-6347-456X; Kita, Noriko/0000-0002-0204-0765;
   Valley, John/0000-0003-3530-2722
FU NASA Astrobiology Institute; NSF [EAR-0509639, EAR-0319230, 0744079];
   DOE [93ER14389]; NASA [NNX09AG39G]; Tawani Foundation
FX We thank the following for assistance: B. Hess, sample preparation and
   polishing; J. Kern, SIMS and profilometer; and J. Fournelle, SEM/EDS. We
   thank C. M. Johnson, B. Beard, S. Moorbath, C. Klein and R. Dymek for
   the Isua samples; and B. Norsted for assistance in curation of
   Hamersley, Transvaal and Biwabik samples. We thank Associate Editor
   Trevor R. Ireland, two anonymous reviewers and A. Schmitt for helpful
   and constructive reviews, C. M. Johnson and H. Xu for helpful comments
   on an earlier version of the manuscript. P. R. H. was supported by the
   NASA Astrobiology Institute, NSF (EAR-0509639, J.W.V.), DOE (93ER14389,
   J.W.V.), NASA (NNX09AG39G, A. M. Davis) and the Tawani Foundation. The
   WiscSIMS lab is partially supported by NSF (EAR-0319230, 0744079). This
   research utilized NSF-supported shared facilities at the University of
   Wisconsin.
NR 83
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U1 3
U2 65
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD OCT 15
PY 2011
VL 75
IS 20
BP 5879
EP 5891
DI 10.1016/j.gca.2011.07.023
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 830EZ
UT WOS:000295641600005
ER

PT J
AU Periyakaruppan, A
   Arumugam, PU
   Meyyappan, M
   Koehne, JE
AF Periyakaruppan, Adaikkappan
   Arumugam, Prabhu U.
   Meyyappan, M.
   Koehne, Jessica E.
TI Detection of ricin using a carbon nanofiber based biosensor
SO BIOSENSORS & BIOELECTRONICS
LA English
DT Article
DE Ricin; Carbon nanofiber; Antibody; Aptamer; Electrochemical impedance
   spectroscopy
ID NANOTUBE NANOELECTRODE ARRAYS; SURFACE-PLASMON RESONANCE; ELECTRODE
   ARRAYS; WARFARE AGENTS; IMMUNOSENSOR; TRENDS
AB We report ricin detection using antibody and aptamer probes immobilized on a nanoelectrode array (NEA) consisting of vertically aligned carbon nanofibers (VACNFs). These biosensor chips are fabricated on a wafer scale using steps common in integrated circuit manufacturing. Electrochemical impedance spectroscopy is used to characterize the detection event and the results indicate that the electron transfer resistance changes significantly after the ricin protein binds to the probe. Further confirmation is obtained from evaluation of the electrode surface by atomic force microscopy which clearly shows a change in height from the bare electrode to the surface bound by the probe-protein. Published by Elsevier B.V.
C1 [Periyakaruppan, Adaikkappan; Arumugam, Prabhu U.; Meyyappan, M.; Koehne, Jessica E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Koehne, JE (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Jessica.E.Koehne@nasa.gov
RI Periyakaruppan, Adaikkappan/B-7398-2013
OI Periyakaruppan, Adaikkappan/0000-0002-0395-6564
FU Texas Southern University; Norfolk State University; NASA URC
   [NNX08BA47A]; Department of Homeland Security [IAA: HSHQDC-08-X-00870]
FX The authors acknowledge Prof. Nader Pourmand and Dr. Paolo Actis of
   University of California Santa Cruz for providing the aptamers used in
   this work and Dr. Olufisayo Jejelowo of Texas Southern University and
   Dr. Govindarajan Ramesh of Norfolk State University for their support.
   Adaikkappan Periyakaruppan is a Postdoctoral Fellow from Texas Southern
   University, Houston, supported by a NASA URC contract to TSU,
   NNX08BA47A. This work was supported in part by the Department of
   Homeland Security through contract IAA: HSHQDC-08-X-00870.
NR 23
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U1 3
U2 63
PU ELSEVIER ADVANCED TECHNOLOGY
PI OXFORD
PA OXFORD FULFILLMENT CENTRE THE BOULEVARD, LANGFORD LANE, KIDLINGTON,
   OXFORD OX5 1GB, OXON, ENGLAND
SN 0956-5663
J9 BIOSENS BIOELECTRON
JI Biosens. Bioelectron.
PD OCT 15
PY 2011
VL 28
IS 1
BP 428
EP 433
DI 10.1016/j.bios.2011.07.061
PG 6
WC Biophysics; Biotechnology & Applied Microbiology; Chemistry, Analytical;
   Electrochemistry; Nanoscience & Nanotechnology
SC Biophysics; Biotechnology & Applied Microbiology; Chemistry;
   Electrochemistry; Science & Technology - Other Topics
GA 830MS
UT WOS:000295661700066
PM 21852102
ER

PT J
AU De Pasquale, M
   Evans, P
   Oates, S
   Page, M
   Zane, S
   Schady, P
   Breeveld, A
   Holland, S
   Still, M
AF De Pasquale, Massimiliano
   Evans, P.
   Oates, S.
   Page, M.
   Zane, S.
   Schady, P.
   Breeveld, A.
   Holland, S.
   Still, M.
TI Can a double component outflow explain the X-ray and optical lightcurves
   of Swift Gamma-Ray Bursts?
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Gamma-Ray Bursts; Relativistic outflow; Multi-component outflow
ID AFTERGLOW LIGHT CURVES; JET BREAKS; THEORETICAL IMPLICATIONS; XRT DATA;
   BEPPOSAX; CATALOG
AB An increasing sample of Gamma-Ray Bursts (GRBs) observed by Swift show evidence of 'chromatic breaks', i.e. breaks that are present in the X-ray but not in the optical. We find that in a significant fraction of these ORB afterglows the X-ray and the optical emission cannot be produced by the same component. We propose that these afterglow lightcurves are the result of a two-component jet, in which both components undergo energy injection for the whole observation and the X-ray break is due to a jet break in the narrow outflow. Bursts with chromatic breaks also explain another surprising finding, the paucity of late achromatic breaks. We propose a model that may explain the behaviour of GRB emission in both X-ray and optical bands. This model can be a radical and noteworthy alternative to the current interpretation for the 'canonical' XRT and UVOT lightcurves, and it bears fundamental implications for GRB physics. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [De Pasquale, Massimiliano; Oates, S.; Page, M.; Zane, S.; Schady, P.; Breeveld, A.; Still, M.] Univ Coll London, Mullard Space Lab, Dorking RH5 6NT, Surrey, England.
   [Evans, P.] Univ Leicester, Leicester LE1 7RH, Leics, England.
   [Holland, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Lab, Holmbury Rd, Dorking RH5 6NT, Surrey, England.
EM mdp@mssl.ucl.ac.uk
FU Royal Society
FX M.D.P. thanks Royal Society for financial support to attend the
   "Frontier of Space Astrophysics - Neutron Star & Gamma-Ray Bursts"
   conference.
NR 13
TC 1
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U1 1
U2 3
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD OCT 15
PY 2011
VL 48
IS 8
BP 1411
EP 1414
DI 10.1016/j.asr.2011.06.006
PG 4
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 825SB
UT WOS:000295301300011
ER

PT J
AU Badavi, FF
   Nealy, JE
   Wilson, JW
AF Badavi, Francis F.
   Nealy, John E.
   Wilson, John W.
TI The Low Earth Orbit validation of a dynamic and anisotropic trapped
   radiation model through ISS measurements
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE LEO; GCR; STS; ISS; GEORAD; HZETRN
ID SPACE RADIATION; ENERGY-SPECTRA; HUMAN PHANTOM; SHUTTLE; ENVIRONMENT;
   PROTONS; STATION; STS-57; BOARD; FLUX
AB The International Space Station (ISS) provides the proving ground for future long duration human activities in space. Ionizing radiation measurements in ISS form the ideal tool for the experimental validation of radiation environmental models, nuclear transport code algorithms and nuclear reaction cross sections. Indeed, prior measurements on the Space Transportation System (STS; Shuttle) have provided vital information impacting both the environmental models and the nuclear transport code development by requiring dynamic models of the Low Earth Orbit (LEO) environment. Previous studies using Computer Aided Design (CAD) models of the evolving ISS configurations with Thermo-Luminescent Detector (TLD) area monitors, demonstrated that computational dosimetry requires environmental models with accurate non-isotropic as well as dynamic behavior, detailed information on rack loading, and an accurate six degree of freedom (DOF) description of ISS trajectory and orientation. It is imperative that we understand ISS exposures dynamically for crew career planning, and insure that the regulatory requirements of keeping exposure as low as reasonably achievable (ALARA) are adequately implemented. This is especially true as ISS nears some form of completion with increasing complexity, resulting in a larger drag coefficient, and requiring operation at higher altitudes with increased exposure rates. In this paper ISS environmental model is configured for 11A (circa mid 2005), and uses non-isotropic and dynamic geomagnetic transmission and trapped proton models. ISS 11A and LEO model validations are important steps in preparation for the design and validation for the next generation manned vehicles. While the described cutoff rigidity, trapped proton and electron formalisms as coded in a package named GEORAD (GEOmagnetic RADiation) and a web interface named OLTARIS (On-line Tool for the Assessment of Radiation in Space) are applicable to the LEO, Medium Earth Orbit (MEO) and Geosynchronous Earth Orbit (GEO) at quiet solar periods, in this report, the validation of the models using available measurements are limited to STS and ISS nominal operational altitudes (300-400 km) range at LEO where the dominant fields within the vehicle are the trapped proton and attenuated Galactic Cosmic Ray (GCR) ions. The described formalism applies to trapped electron at LEO, M DO and GEO as well. Due to the scarcity of available electron measurements, the trapped electron capabilities of the GEORAD are not discussed in this report, but are accessible through OLTARIS web interface. GEORAD and OLTARIS interests are in the study of long term effects (i.e. a meaningful portion of solar cycle). Therefore, GEORAD does not incorporate any short term external field contribution due to solar activity. Finally, we apply these environmental models to selected target points within ISS 6A (circa early 2001), 7A (circa late 2001), and 11 A during its passage through the South Atlantic Anomaly (SAA) to assess the validity of the environmental models at ISS altitudes. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Badavi, Francis F.] Christopher Newport Univ, OSP, Newport News, VA 23606 USA.
   [Nealy, John E.] Old Dominion Univ, Norfolk, VA 23529 USA.
   [Wilson, John W.] NASA, Langley Res Ctr DRA, Hampton, VA 23681 USA.
RP Badavi, FF (reprint author), Christopher Newport Univ, OSP, 1 Univ Pl, Newport News, VA 23606 USA.
EM francis.f.badavi@nasa.gov; John.e.nealy@nasa.gov; jwilson61@cox.net
NR 49
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U1 1
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD OCT 15
PY 2011
VL 48
IS 8
BP 1441
EP 1458
DI 10.1016/j.asr.2011.06.009
PG 18
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 825SB
UT WOS:000295301300015
ER

PT J
AU Raj, SV
AF Raj, S. V.
TI Microstructural characterization of metal foams: An examination of the
   applicability of the theoretical models for modeling foams (vol 528, pg
   5289, 2011)
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
   MICROSTRUCTURE AND PROCESSING
LA English
DT Correction
C1 NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
RP Raj, SV (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, MS 106-5,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM sai.v.raj@nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD OCT 15
PY 2011
VL 528
IS 27
BP 8041
EP 8041
DI 10.1016/j.msea.2011.07.014
PG 1
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
   Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
   Metallurgical Engineering
GA 823FI
UT WOS:000295107500030
ER

PT J
AU Lee, JE
   Lintner, BR
   Boyce, CK
   Lawrence, PJ
AF Lee, Jung-Eun
   Lintner, Benjamin R.
   Boyce, C. Kevin
   Lawrence, Peter J.
TI Land use change exacerbates tropical South American drought by sea
   surface temperature variability
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID AMAZON BASIN; CLIMATE-CHANGE; RAINFALL; PATTERNS; ATLANTIC; FORESTS;
   CONSEQUENCES; SIMULATION; RESPONSES; IMPACTS
AB Observations of tropical South American precipitation over the last three decades indicate an increasing rainfall trend to the north and a decreasing trend to the south. Given that tropical South America has experienced significant land use change over the same period, it is of interest to assess the extent to which changing land use may have contributed to the precipitation trends. Simulations of the National Center for Atmospheric Research Community Atmosphere Model (NCARCAM3) analyzed here suggest a non-negligible impact of land use on this precipitation behavior. While forcing the model by imposed historical sea surface temperatures (SSTs) alone produces a plausible north-south precipitation dipole over South America, NCAR CAM substantially underestimates the magnitude of the observed southern decrease in rainfall unless forcing associated with human-induced land use change is included. The impact of land use change on simulated precipitation occurs primarily during the local dry season and in regions of relatively low annual-mean rainfall, as the incidence of very low monthly-mean accumulations (<10 mm/month) increases significantly when land use change is imposed. Land use change also contributes to the simulated temperature increase by shifting the surface turbulent flux partitioning to favor sensible over latent heating. Moving forward, continuing pressure from deforestation in tropical South America will likely increase the occurrence of significant drought beyond what would be expected by anthropogenic warming alone and in turn compound biodiversity decline from habitat loss and fragmentation. Citation: Lee, J.-E., B. R. Lintner, C. K. Boyce, and P. J. Lawrence (2011), Land use change exacerbates tropical South American drought by sea surface temperature variability, Geophys. Res. Lett., 38, L19706, doi:10.1029/2011GL049066.
C1 [Lee, Jung-Eun] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Lintner, Benjamin R.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA.
   [Boyce, C. Kevin] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
   [Lawrence, Peter J.] Natl Ctr Atmospher Res, TSS, CGD, Boulder, CO 80307 USA.
RP Lee, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-501, Pasadena, CA 91109 USA.
EM jung-eun.lee@jpl.nasa.gov
RI Lee, Jung-Eun/F-8981-2012
FU National Science Foundation [EAR-090919, AGS-1035968]; New Jersey
   Agricultural Experiment Station Hatch [NJ07102]
FX We thank I. Fung, T. Kubar, and R. Pierrehumbert for providing many
   useful suggestions for the improvement of the manuscript and also thank
   the researchers who made GIMMS NDVI, GPCP precipitation, GHCN
   temperature, and HadSST data available. The runs were performed at
   NERSC. JEL acknowledges support from National Science Foundation grant
   EAR-090919. BRL acknowledges support from National Science Foundation
   grant AGS-1035968 and New Jersey Agricultural Experiment Station Hatch
   grant NJ07102.
NR 41
TC 25
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U1 2
U2 28
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 OCT 14
PY 2011
VL 38
AR L19706
DI 10.1029/2011GL049066
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 834QB
UT WOS:000295976500003
ER

PT J
AU Kato, S
   Rose, FG
   Sun-Mack, S
   Miller, WF
   Chen, Y
   Rutan, DA
   Stephens, GL
   Loeb, NG
   Minnis, P
   Wielicki, BA
   Winker, DM
   Charlock, TP
   Stackhouse, PW
   Xu, KM
   Collins, WD
AF Kato, Seiji
   Rose, Fred G.
   Sun-Mack, Sunny
   Miller, Walter F.
   Chen, Yan
   Rutan, David A.
   Stephens, Graeme L.
   Loeb, Norman G.
   Minnis, Patrick
   Wielicki, Bruce A.
   Winker, David M.
   Charlock, Thomas P.
   Stackhouse, Paul W., Jr.
   Xu, Kuan-Man
   Collins, William D.
TI Improvements of top-of-atmosphere and surface irradiance computations
   with CALIPSO-, CloudSat-, and MODIS-derived cloud and aerosol properties
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM
   INSTRUMENT; TERRA SATELLITE; INPUT DATA; DATA SETS; PART II; BUDGET;
   PARAMETERIZATION; VARIABILITY
AB One year of instantaneous top-of-atmosphere (TOA) and surface shortwave and longwave irradiances are computed using cloud and aerosol properties derived from instruments on the A-Train Constellation: the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) on the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) satellite, the CloudSat Cloud Profiling Radar (CPR), and the Aqua Moderate Resolution Imaging Spectrometer (MODIS). When modeled irradiances are compared with those computed with cloud properties derived from MODIS radiances by a Clouds and the Earth's Radiant Energy System (CERES) cloud algorithm, the global and annual mean of modeled instantaneous TOA irradiances decreases by 12.5 W m(-2) (5.0%) for reflected shortwave and 2.5 W m(-2) (1.1%) for longwave irradiances. As a result, the global annual mean of instantaneous TOA irradiances agrees better with CERES-derived irradiances to within 0.5 W m(-2) (out of 237.8 W m(-2)) for reflected shortwave and 2.6 W m(-2) (out of 240.1 W m(-2)) for longwave irradiances. In addition, the global annual mean of instantaneous surface downward longwave irradiances increases by 3.6 W m(-2) (1.0%) when CALIOP- and CPR-derived cloud properties are used. The global annual mean of instantaneous surface downward shortwave irradiances also increases by 8.6 W m(-2) (1.6%), indicating that the net surface irradiance increases when CALIOP- and CPR-derived cloud properties are used. Increasing the surface downward longwave irradiance is caused by larger cloud fractions (the global annual mean by 0.11, 0.04 excluding clouds with optical thickness less than 0.3) and lower cloud base heights (the global annual mean by 1.6 km). The increase of the surface downward longwave irradiance in the Arctic exceeds 10 W m(-2) (similar to 4%) in winter because CALIOP and CPR detect more clouds in comparison with the cloud detection by the CERES cloud algorithm during polar night. The global annual mean surface downward longwave irradiance of 345.4 W m(-2) is estimated by combining the modeled instantaneous surface longwave irradiance computed with CALIOP and CPR cloud profiles with the global annual mean longwave irradiance from the CERES product (AVG), which includes the diurnal variation of the irradiance. The estimated bias error is -1.5 W m(-2) and the uncertainty is 6.9 W m(-2). The uncertainty is predominately caused by the near-surface temperature and column water vapor amount uncertainties.
C1 [Kato, Seiji; Loeb, Norman G.; Minnis, Patrick; Wielicki, Bruce A.; Winker, David M.; Charlock, Thomas P.; Stackhouse, Paul W., Jr.; Xu, Kuan-Man] NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23668 USA.
   [Rose, Fred G.; Sun-Mack, Sunny; Miller, Walter F.; Chen, Yan; Rutan, David A.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
   [Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Collins, William D.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
RP Kato, S (reprint author), NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23668 USA.
EM seiji.kato@nasa.gov
RI Xu, Kuan-Man/B-7557-2013; Collins, William/J-3147-2014; Minnis,
   Patrick/G-1902-2010; 
OI Xu, Kuan-Man/0000-0001-7851-2629; Collins, William/0000-0002-4463-9848;
   Minnis, Patrick/0000-0002-4733-6148; Rose, Fred G/0000-0003-0769-0772
FU NASA
FX We thank Bing Lin, Tristan L'Ecuyer, and Stefan Kinne for useful
   discussions and Amber Richards for proof reading the manuscript. The
   work was supported by the NASA Energy Water Cycle Study (NEWS) project.
   Also two of the authors (S. K. and P. M.) received support from the NASA
   cryosphere IPY program for this study.
NR 63
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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 OCT 14
PY 2011
VL 116
AR D19209
DI 10.1029/2011JD016050
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835DL
UT WOS:000296014500005
ER

PT J
AU Yoshimura, K
   Frankenberg, C
   Lee, J
   Kanamitsu, M
   Worden, J
   Rockmann, T
AF Yoshimura, Kei
   Frankenberg, Christian
   Lee, Jeonghoon
   Kanamitsu, Masao
   Worden, John
   Rockmann, Thomas
TI Comparison of an isotopic atmospheric general circulation model with new
   quasi-global satellite measurements of water vapor isotopologues
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID QUANTITATIVE-ANALYSIS; PRECIPITATION; DELTA-O-18; CYCLE; O-18; HDO;
   FRACTIONATION; STRATOSPHERE; EVAPORATION; SIMULATION
AB We performed an intensive comparison of an isotope-incorporated atmospheric general circulation model with vapor isotopologue ratio observation data by two quasi-global satellite sensors in preparation for data assimilation of water isotope ratios. A global Isotope-incorporated Global Spectral Model simulation nudged toward the reanalysis wind field, atmospheric total column data from Scanning Imaging Absorption Spectrometer for Atmospheric Cartography (SCIAMACHY) on Envisat, and midtropospheric (800 to 500 hPa) data from Tropospheric Emission Spectrometer (TES) on Aura were used. For the mean climatological delta D of both the total atmospheric column and the midtroposphere layer, the model reproduced their geographical variabilities quite well. There is, however, some degree of underestimation of the latitudinal gradient (higher delta D in the tropics and lower delta D in midlatitudes) compared to the SCIAMACHY data, whereas there is generally less disagreement except lower delta D over the Maritime Continent compared to the TES data. It was also found that the two satellite products have different relationships between water vapor amount and isotopic composition. Particularly, atmospheric column mean delta D, which is dominated by lower-tropospheric vapor, closely follows the fractionation pattern of a typical Rayleigh-type "rain out" process, whereas in the midtroposphere the relationship between isotopic composition and vapor amount is affected by a "mixing" process. This feature is not reproduced by the model, where the relationships between delta D and the vapor are similar to each other for the atmospheric column and midtroposphere. Comparing on a shorter time scale, it becomes clear that the data situation for future data assimilation for total column delta D is most favorable for tropical and subtropical desert areas (i.e., Sahel, southern Africa, mideastern Asia, Gobi, Australia, and the southwest United States), whereas the available midtropospheric delta D observations cover wider regions, particularly over tropical to subtropical oceans.
C1 [Yoshimura, Kei] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan.
   [Frankenberg, Christian] Univ Tokyo, Inst Ind Sci, Tokyo, Japan.
   [Frankenberg, Christian; Worden, John] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Lee, Jeonghoon] Korea Polar Res Inst, Inchon 406840, South Korea.
   [Kanamitsu, Masao] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
   [Rockmann, Thomas] Inst Marine & Atmospher Res Utrecht, NL-3508 Utrecht, Netherlands.
RP Yoshimura, K (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan.
EM kei@aori.u-tokyo.ac.jp
RI Yoshimura, Kei/F-2041-2010; Lee, Jeonghoon/E-8116-2010; Rockmann,
   Thomas/F-4479-2015; Frankenberg, Christian/A-2944-2013
OI Yoshimura, Kei/0000-0002-5761-1561; Lee, Jeonghoon/0000-0002-1256-4431;
   Rockmann, Thomas/0000-0002-6688-8968; Frankenberg,
   Christian/0000-0002-0546-5857
FU Japan Society for the Promotion of Science (JSPS) [23686071]; California
   Energy Commission; California Climate Change Center [MGC-04-04]; NOAA
   [NA17RJ1231]
FX A part of this research was funded by the Japan Society for the
   Promotion of Science (JSPS) grant 23686071. The numerical simulations
   were performed with computing resources at the Center for Observations
   and Prediction at Scripps (COMPAS) and at TeraGrid. Part of this work
   was also funded by the California Energy Commission Public Interest
   Energy Research (PIER) program, which supports the California Climate
   Change Center (award MGC-04-04) and NOAA (NA17RJ1231). The views
   expressed herein are those of the authors and do not necessarily reflect
   the views of NOAA. We would like to thank J. Roads for his encouragement
   in the beginning of this study. The assistance of Ms. D. Boomer in
   refining the writing is appreciated. The authors thank all the comments
   from two reviewers including Matthias Schneider.
NR 53
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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 OCT 14
PY 2011
VL 116
AR D19118
DI 10.1029/2011JD016035
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835DL
UT WOS:000296014500004
ER

PT J
AU Jackman, CM
   Slavin, JA
   Cowley, SWH
AF Jackman, C. M.
   Slavin, J. A.
   Cowley, S. W. H.
TI Cassini observations of plasmoid structure and dynamics: Implications
   for the role of magnetic reconnection in magnetospheric circulation at
   Saturn
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GEOMAGNETIC TAIL; FIELD; MAGNETOTAIL; EVOLUTION; FLOWS; CYCLE; HST
AB We survey the Cassini magnetometer data during the deep tail orbits in 2006, and find 34 direct encounters with plasmoids. They occur as single, isolated events but also in groups of two or more plasmoids as is frequently observed at Earth. We show a case study example of three such plasmoids over three hours, where we estimate an upper limit of 5.68 GWb of flux closure, and derive a reconnection rate over this interval of 526 kV. We show the results of a superposed epoch analysis of all 34 plasmoids indicating that, on average, plasmoids at Saturn are similar to 8 min in duration and they tend toward a loop-like, as opposed to flux rope-like topology, with little or no axial core magnetic field. Our analysis shows that plasmoids at Saturn are followed by an extended interval of the post-plasmoid plasma sheet (PPPS) lasting similar to 58 min. The average open magnetic flux disconnected by the continued reconnection following plasmoid formation that creates the PPPS is similar to 3 GWb. We calculate expected recurrence rates for plasmoids, and compare these with a derived observational recurrence rate of one plasmoid every similar to 2.4 days, explaining the reasons why the spacecraft has not observed as many plasmoids as we predict will be released. We conclude that the Cassini magnetometer measurements require a combination of Vasyliunas-type closed-flux plasma sheet and Dungey-type open-flux lobe reconnection to account for the observed properties of the plasmoids and PPPS in Saturn's magnetotail.
C1 [Jackman, C. M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
   [Slavin, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Cowley, S. W. H.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Jackman, CM (reprint author), UCL, Dept Phys & Astron, Gower Pl, London WC1E 6BT, England.
EM caitriona.jackman@ucl.ac.uk
RI Slavin, James/H-3170-2012; 
OI Slavin, James/0000-0002-9206-724X; Jackman,
   Caitriona/0000-0003-0635-7361
FU Science and Technology Facilities Council (STFC) [ST/H002480/1];
   Leverhulme Trust
FX C.M.J. would like to thank Neal Powell at Imperial for artwork. Work at
   Imperial College London was funded by the Science and Technology
   Facilities Council (STFC). We acknowledge M. K. Dougherty for provision
   of the Cassini magnetometer data and S. Kellock and the team at Imperial
   College London for MAG data processing. C.M.J. and J.A.S. acknowledge
   useful discussions with the International Space Science Institute (ISSI)
   "Dynamics of Planetary Magnetotails" team led by C.M.J. C.M.J. 's work
   at UCL is funded through a Leverhulme Trust Early Career Fellowship.
   Work at the University of Leicester was supported by STFC grant
   ST/H002480/1.
NR 37
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U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 14
PY 2011
VL 116
AR A10212
DI 10.1029/2011JA016682
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 834TM
UT WOS:000295987000002
ER

PT J
AU Avramov, A
   Ackerman, AS
   Fridlind, AM
   van Diedenhoven, B
   Botta, G
   Aydin, K
   Verlinde, J
   Korolev, AV
   Strapp, JW
   McFarquhar, GM
   Jackson, R
   Brooks, SD
   Glen, A
   Wolde, M
AF Avramov, Alexander
   Ackerman, Andrew S.
   Fridlind, Ann M.
   van Diedenhoven, Bastiaan
   Botta, Giovanni
   Aydin, Kultegin
   Verlinde, Johannes
   Korolev, Alexei V.
   Strapp, J. Walter
   McFarquhar, Greg M.
   Jackson, Robert
   Brooks, Sarah D.
   Glen, Andrew
   Wolde, Mengistu
TI Toward ice formation closure in Arctic mixed-phase boundary layer clouds
   during ISDAC
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LARGE-EDDY SIMULATIONS; PARTICLE TERMINAL VELOCITIES; GENERAL
   HYDRODYNAMIC THEORY; MODEL SIMULATIONS; STRATIFORM CLOUDS; RESOLVING
   SIMULATIONS; MARINE STRATOCUMULUS; AEROSOL-PARTICLES; DOPPLER SPECTRA;
   WAVE CLOUD
AB A modeling study of a low-lying mixed-phase cloud layer observed on 8 April 2008 during the Indirect and Semi-Direct Aerosol Campaign is presented. Large-eddy simulations with size-resolved microphysics were used to test the hypothesis that heterogeneous ice nucleus (IN) concentrations measured above cloud top can account for observed ice concentrations, while also matching ice size distributions, radar reflectivities, and mean Doppler velocities. The conditions for the case are favorable for the hypothesis: springtime IN concentrations are high in the Arctic, the predominant ice habit falls slowly, and overlying IN concentrations were greater than ice particle number concentrations. Based on particle imagery, we considered two dendrite types, broad armed (high density) and stellar (low density), in addition to high and low density aggregates. Two simulations with low-density aggregates reproduced observations best overall: one in which IN concentrations aloft were increased fourfold (as could have been present above water saturation) and another in which initial IN concentrations were vertically uniform. A key aspect of the latter was an IN reservoir under the well-mixed cloud layer: as the simulations progressed, the reservoir IN slowly mixed upward, helping to maintain ice concentrations close to those observed. Given the uncertainties of the measurements and parameterizations of the microphysical processes embedded in the model, we found agreement between simulated and measured ice number concentrations in most of the simulations, in contrast with previous modeling studies of Arctic mixed-phase clouds, which typically show a large discrepancy when IN are treated prognostically and constrained by measurements.
C1 [Avramov, Alexander; van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
   [Ackerman, Andrew S.; Fridlind, Ann M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Botta, Giovanni; Aydin, Kultegin] Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA.
   [Botta, Giovanni; Verlinde, Johannes] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
   [Brooks, Sarah D.; Glen, Andrew] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
   [McFarquhar, Greg M.; Jackson, Robert] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
   [Korolev, Alexei V.; Strapp, J. Walter] Environm Canada, Sci & Technol Branch, Toronto, ON M3H 5T4, Canada.
   [Wolde, Mengistu] CNR, Flight Res Lab, Ottawa, ON K1A 0R6, Canada.
RP Avramov, A (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave,Rm 54-1415, Cambridge, MA 02139 USA.
EM lz4ax@mit.edu
RI Ackerman, Andrew/D-4433-2012; van Diedenhoven, Bastiaan/A-2002-2013; 
OI Ackerman, Andrew/0000-0003-0254-6253; van Diedenhoven,
   Bastiaan/0000-0001-5622-8619; McFarquhar, Greg/0000-0003-0950-0135
FU DOE Office of Science [DE-AC02-05CH11231]; DOE Office of Science, Office
   of Biological and Environmental Research [DE-AI02-06ER64173,
   DE-AI02-08ER64547]; NASA
FX We thank Steven Ghan (ISDAC project scientist) and the flight crew of
   the NRC Convair-580 for making these measurements possible. We also
   thank Peter Liu and Michael Earle of Environment Canada for providing
   the best-estimate aerosol size distribution for this case. We are
   grateful to the three anonymous reviewers for helpful comments. This
   research used resources of the National Energy Research Scientific
   Computing Center, which is supported by the DOE Office of Science under
   contract DE-AC02-05CH11231. This work was supported by the DOE Office of
   Science, Office of Biological and Environmental Research, through
   Interagency Agreements DE-AI02-06ER64173 and DE-AI02-08ER64547, and by
   the NASA Radiation Sciences Program. ARM data are made available through
   the U.S. Department of Energy as part of the Atmospheric Radiation
   Measurement Program.
NR 85
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U1 1
U2 33
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 OCT 13
PY 2011
VL 116
AR D00T08
DI 10.1029/2011JD015910
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 971AC
UT WOS:000306172900005
ER

PT J
AU Morlighem, M
   Rignot, E
   Seroussi, H
   Larour, E
   Ben Dhia, H
   Aubry, D
AF Morlighem, M.
   Rignot, E.
   Seroussi, H.
   Larour, E.
   Ben Dhia, H.
   Aubry, D.
TI A mass conservation approach for mapping glacier ice thickness
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GREENLAND; TOPOGRAPHY
AB The traditional method for interpolating ice thickness data from airborne radar sounding surveys onto regular grids is to employ geostatistical techniques such as kriging. While this approach provides continuous maps of ice thickness, it generates products that are not consistent with ice flow dynamics and are impractical for high resolution ice flow simulations. Here, we present a novel approach that combines sparse ice thickness data collected by airborne radar sounding profilers with high resolution swath mapping of ice velocity derived from satellite synthetic-aperture interferometry to obtain a high resolution map of ice thickness that conserves mass and minimizes the departure from observations. We apply this approach to the case of Nioghalvfjerdsfjorden (79North) Glacier, a major outlet glacier in northeast Greenland that has been relatively stable in recent decades. The results show that our mass conserving method removes the anomalies in mass flux divergence, yields interpolated data that are within about 5% of the original data, and produces thickness maps that are directly usable in high spatial-resolution, high-order ice flow models. We discuss the application of this method to the broad and detailed radar surveys of ice sheet and glacier thickness. Citation: Morlighem, M., E. Rignot, H. Seroussi, E. Larour, H. Ben Dhia, and D. Aubry (2011), A mass conservation approach for mapping glacier ice thickness, Geophys. Res. Lett., 38, L19503, doi:10.1029/2011GL048659.
C1 [Morlighem, M.; Rignot, E.; Seroussi, H.; Larour, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Morlighem, M.; Seroussi, H.; Ben Dhia, H.; Aubry, D.] Ecole Cent Paris, Lab MSSMat, CNRS, UMR 8579, F-92295 Chatenay Malabry, France.
   [Rignot, E.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
RP Morlighem, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-227, Pasadena, CA 91109 USA.
EM Mathieu.Morlighem@jpl.nasa.gov
RI Rignot, Eric/A-4560-2014; Morlighem, Mathieu/O-9942-2014
OI Rignot, Eric/0000-0002-3366-0481; Morlighem, Mathieu/0000-0001-5219-1310
FU NASA
FX This work was performed at the Jet Propulsion Laboratory, California
   Institute of Technology, at the Department of Earth System Science,
   University of California Irvine, and at Laboratoire MSSMat, Ecole
   Centrale Paris, under a contract with the NASA Cryospheric Sciences
   Program. The authors thank two anonymous reviewers for helpful and
   insightful comments. We would also like to acknowledge the use of data
   and/or data products from CReSIS and OIB, which greatly helped to
   evaluate our method.
NR 17
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U1 0
U2 16
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 OCT 13
PY 2011
VL 38
AR L19503
DI 10.1029/2011GL048659
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 855CR
UT WOS:000297541700001
ER

PT J
AU Makishima, T
   Hochman, L
   Armstrong, P
   Rosenberger, E
   Ridley, R
   Woo, M
   Perachio, A
   Wood, S
AF Makishima, Tomoko
   Hochman, Lara
   Armstrong, Patrick
   Rosenberger, Eric
   Ridley, Ryan
   Woo, Minna
   Perachio, Adrian
   Wood, Scott
TI Inner ear dysfunction in caspase-3 deficient mice
SO BMC NEUROSCIENCE
LA English
DT Article
ID PROGRAMMED CELL-DEATH; HIGHLY MUTABLE LOCUS; SENSORY EPITHELIA; C57BL/6
   MICE; MOUSE; DEFECTS; MORPHOGENESIS; APOPTOSIS; GENE; HINDBRAIN
AB Background: Caspase-3 is one of the most downstream enzymes activated in the apoptotic pathway. In caspase-3 deficient mice, loss of cochlear hair cells and spiral ganglion cells coincide closely with hearing loss. In contrast with the auditory system, details of the vestibular phenotype have not been characterized. Here we report the vestibular phenotype and inner ear anatomy in the caspase-3 deficient (Casp3(-/-)) mouse strain.
   Results: Average ABR thresholds of Casp3(-/-) mice were significantly elevated (P < 0.05) compared to Casp3(+/-) mice and Casp3(+/+) mice at 3 months of age. In DPOAE testing, distortion product 2F1-F2 was significantly decreased (P < 0.05) in Casp3(-/-) mice, whereas Casp3(+/-) and Casp3(+/+) mice showed normal and comparable values to each other. Casp3(-/-) mice were hyperactive and exhibited circling behavior when excited. In lateral canal VOR testing, Casp3(-/-) mice had minimal response to any of the stimuli tested, whereas Casp3(+/-) mice had an intermediate response compared to Casp3(+/+) mice. Inner ear anatomical and histological analysis revealed gross hypomorphism of the vestibular organs, in which the main site was the anterior semicircular canal. Hair cell numbers in the anterior-and lateral crista, and utricle were significantly smaller in Casp3(-/-) mice whereas the Casp3(+/-) and Casp3(+/+) mice had normal hair cell numbers.
   Conclusions: These results indicate that caspase-3 is essential for correct functioning of the cochlea as well as normal development and function of the vestibule.
C1 [Makishima, Tomoko; Ridley, Ryan; Perachio, Adrian; Wood, Scott] Univ Texas Med Branch, Dept Otolaryngol, Galveston, TX USA.
   [Hochman, Lara; Armstrong, Patrick; Rosenberger, Eric] Univ Texas Med Branch, Sch Med, Galveston, TX USA.
   [Woo, Minna] Univ Toronto, Ontario Canc Inst, Dept Med, Toronto, ON, Canada.
   [Wood, Scott] NASA, Johnson Space Ctr, Univ Space Res Assoc, Houston, TX USA.
RP Makishima, T (reprint author), Univ Texas Med Branch, Dept Otolaryngol, Galveston, TX USA.
EM tomakish@utmb.edu
NR 43
TC 15
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U1 0
U2 2
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2202
J9 BMC NEUROSCI
JI BMC Neurosci.
PD OCT 12
PY 2011
VL 12
AR 102
DI 10.1186/1471-2202-12-102
PG 9
WC Neurosciences
SC Neurosciences & Neurology
GA 842ZA
UT WOS:000296639900001
PM 21988729
ER

PT J
AU Chen, WT
   Woods, CP
   Li, JLF
   Waliser, DE
   Chern, JD
   Tao, WK
   Jiang, JH
   Tompkins, AM
AF Chen, Wei-Ting
   Woods, Christopher P.
   Li, Jui-Lin F.
   Waliser, Duane E.
   Chern, Jiun-Dar
   Tao, Wei-Kuo
   Jiang, Jonathan H.
   Tompkins, Adrian M.
TI Partitioning CloudSat ice water content for comparison with upper
   tropospheric ice in global atmospheric models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPICAL CIRRUS; RADIATIVE-TRANSFER; RADAR; MICROPHYSICS; CLIMATE;
   SYSTEM; PARAMETERIZATION; PRECIPITATION; SIMULATIONS; RETRIEVALS
AB The ice cloud estimates in current global models exhibit significant inconsistency, resulting in a significant amount of uncertainties in climate forecasting. Vertically resolved ice water content (IWC) is recently available from new satellite products, such as CloudSat, providing important observational constraints for evaluating the global models. To account for the varied nature of the model parameterization schemes, it is valuable to develop methods to distinguish the cloud versus precipitating ice components from the remotely sensed estimates in order to carry out meaningful model-data comparisons. The present study develops a new technique that partitions CloudSat total IWC into small and large ice hydrometeors, using the ice particle size distribution (PSD) parameters provided by the retrieval algorithm. The global statistics of CloudSat-retrieved PSD are analyzed for the filtered subsets on the basis of convection and precipitation flags to identify appropriate particle size separation. Results are compared with previous partitioning estimates and suggest that the small particles contribute to similar to 25-45% of the global mean total IWC in the upper to middle troposphere. Sensitivity measures with respect to the PSD parameters and the retrieval algorithm are presented. The current estimates are applied to evaluate the IWC estimates from the European Centre for Medium-Range Weather Forecasts model and the finite-volume multiscale modeling framework model, pointing to specific areas of potential model improvements. These results are discussed in terms of applications to model diagnostics, providing implications for reducing the uncertainty in the model representation of cloud feedback and precipitation.
C1 [Chen, Wei-Ting; Woods, Christopher P.; Li, Jui-Lin F.; Waliser, Duane E.; Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Chern, Jiun-Dar; Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Tompkins, Adrian M.] Abdus Salam Int Ctr Theoret Phys, I-34152 Trieste, Italy.
   [Tompkins, Adrian M.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
RP Chen, WT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM annechen@caltech.edu
RI Tompkins, Adrian/N-6472-2013; Chen, Wei-Ting/A-4476-2012
OI Tompkins, Adrian/0000-0003-0975-6691; Chen, Wei-Ting/0000-0002-9292-0933
FU NASA
FX This research was carried out at the Jet Propulsion Laboratory,
   California Institute of Technology, under a contract with NASA. It is
   supported by the NASA CloudSat program. CloudSat data were provided by
   the NASA CloudSat project through Colorado State University.
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TC 17
Z9 17
U1 0
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 OCT 12
PY 2011
VL 116
AR D19206
DI 10.1029/2010JD015179
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835DK
UT WOS:000296014400001
ER

PT J
AU Yorks, JE
   Hlavka, DL
   Vaughan, MA
   McGill, MJ
   Hart, WD
   Rodier, S
   Kuehn, R
AF Yorks, John E.
   Hlavka, Dennis L.
   Vaughan, Mark A.
   McGill, Matthew J.
   Hart, William D.
   Rodier, Sharon
   Kuehn, Ralph
TI Airborne validation of cirrus cloud properties derived from CALIPSO
   lidar measurements: Spatial properties
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ALGORITHM; MODEL; PERFORMANCE; RETRIEVAL; RETURNS; MODIS
AB The Cloud-Aerosol Lidar Infrared Pathfinder Satellite Observations (CALIPSO) satellite was successfully launched in 2006 and has provided an unprecedented opportunity to study cloud and aerosol layers using range-resolved laser remote sensing. Dedicated validation flights were conducted using the airborne Cloud Physics Lidar (CPL) to validate the CALIPSO Level 1 and 2 data products. This paper presents results from coincident CALIPSO and CPL measurements of ice cloud spatial properties. Flight segment case studies are shown as well as statistics for all coincident measurements during the CALIPSO-CloudSat Validation Experiment (CC-VEX). CALIPSO layer detection algorithms for cirrus clouds are reliable in comparison with CPL, with best agreement occurring during nighttime coincident segments when the signal-to-noise ratio (SNR) of both instruments is greatest. However, the two instruments disagree on ice cloud spatial properties in two distinct cases. CALIPSO experiences less sensitivity to optically thin cirrus due to lower SNR when compared to CPL data at identical spatial scales. The incorporation of extended spatial averaging in the CALIPSO layer detection algorithm succeeds in detecting the optically thin cirrus, but the averaging process occasionally results in spatial smearing, both horizontally and vertically, of broken cirrus clouds. The second disparity occurs because, in contrast to CPL, multiple scattering contributes significantly to CALIPSO lidar measurements of cirrus clouds. As a result, the CALIPSO signal penetrates deeper into opaque cirrus clouds, and in these cases CALIPSO will report lower apparent cloud base altitudes than CPL.
C1 [Yorks, John E.; Hlavka, Dennis L.; McGill, Matthew J.; Hart, William D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Yorks, John E.; Hlavka, Dennis L.; Hart, William D.; Rodier, Sharon] Sci Syst & Applicat Inc, Lanham, MD USA.
   [Vaughan, Mark A.; Rodier, Sharon] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Kuehn, Ralph] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA.
RP Yorks, JE (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA.
EM john.e.yorks@nasa.gov
RI McGill, Matthew/D-8176-2012; jingjing, cai/M-2687-2013; 
OI Hlavka, Dennis/0000-0002-2976-7243
FU NASA
FX NASA's Radiation Sciences Program funded this study. Special thanks go
   to all the members of the CALIPSO science team for making the instrument
   data available.
NR 37
TC 17
Z9 17
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 12
PY 2011
VL 116
AR D19207
DI 10.1029/2011JD015942
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835DK
UT WOS:000296014400005
ER

PT J
AU Roberts, CD
   LeGrande, AN
   Tripati, AK
AF Roberts, Christopher D.
   LeGrande, Allegra N.
   Tripati, Aradhna K.
TI Sensitivity of seawater oxygen isotopes to climatic and tectonic
   boundary conditions in an early Paleogene simulation with GISS ModelE-R
SO PALEOCEANOGRAPHY
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; EOCENE THERMAL MAXIMUM; CARBON-DIOXIDE
   CONCENTRATIONS; SEA-SURFACE TEMPERATURES; ATMOSPHERE-OCEAN MODEL;
   PLANKTONIC-FORAMINIFERA; GLOBAL CLIMATE; MIDDLE EOCENE; DRAKE PASSAGE;
   ARCTIC-OCEAN
AB An isotope-enabled ocean-atmosphere general circulation model (GISS ModelE-R) is used to estimate the spatial gradients of the oxygen isotopic composition of seawater (delta O-18(sw), where delta is the deviation from a known reference material in per mil) during the early Paleogene (45-65 Ma). Understanding the response of delta O-18(sw) to changes in climatic and tectonic boundary conditions is important because records of carbonate delta O-18 document changes in hydrology, as well as changes in temperature and global ice-volume. We present results from an early Paleogene configuration of ModelE-R which indicate that spatial gradients of surface ocean delta O-18(sw) during this period could have been significantly different to those in the modern ocean. The differences inferred from ModelE-R are sufficient to change early Paleogene sea surface temperature estimates derived from primary carbonate delta O-18 signatures by more than +/- 2 degrees C in large areas of the ocean. In the North Atlantic, Indian, and Southern Oceans, the differences in delta O-18(sw) inferred from our simulation with ModelE-R are in direct contrast with those from another delta O-18-tracing model study which used different, but equally plausible, early Paleogene boundary conditions. The large differences in delta O-18(sw) between preindustrial and early Paleogene simulations, and between models, emphasizes the sensitivity of delta O-18(sw) to climatic and tectonic boundary conditions. For this reason, absolute estimates of Eocene/Paleocene temperature derived from carbonate delta O-18 alone are likely to have larger uncertainties than are usually assumed.
C1 [Roberts, Christopher D.; Tripati, Aradhna K.] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England.
   [LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
   [Tripati, Aradhna K.] Univ Calif Los Angeles, Inst Environm, Los Angeles, CA 90095 USA.
   [Tripati, Aradhna K.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
   [Tripati, Aradhna K.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
RP Roberts, CD (reprint author), Met Off Hadley Ctr, Fitzroy Rd, Exeter EX1 3PB, Devon, England.
EM roberts.cd@gmail.com
RI Tripati, Aradhna/C-9419-2011; Roberts, Christopher/F-6197-2011;
   LeGrande, Allegra/D-8920-2012
OI Tripati, Aradhna/0000-0002-1695-1754; LeGrande,
   Allegra/0000-0002-5295-0062
FU NSF [ATM 07-53868]; NERC [NER/S/A/2006/14070]; UCLA Division of Physical
   Sciences; Magdalene College
FX We thank NASA GISS for institutional support. A.N.L. was supported by
   NSF ATM 07-53868, C. D. R. was supported by a NERC studentship
   (NER/S/A/2006/14070), and A. K. T. was supported by the UCLA Division of
   Physical Sciences, NERC, and Magdalene College. We thank an anonymous
   reviewer and G. A. Schmidt for helpful comments on previous versions of
   this work and K. Bice and J. Sewall for providing us with gridded data
   for the model boundary conditions.
NR 112
TC 9
Z9 9
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0883-8305
EI 1944-9186
J9 PALEOCEANOGRAPHY
JI Paleoceanography
PD OCT 12
PY 2011
VL 26
AR PA4203
DI 10.1029/2010PA002025
PG 16
WC Geosciences, Multidisciplinary; Oceanography; Paleontology
SC Geology; Oceanography; Paleontology
GA 834TF
UT WOS:000295986300001
ER

PT J
AU Abbasi, R
   Abdou, Y
   Abu-Zayyad, T
   Adams, J
   Aguilar, JA
   Ahlers, M
   Altmann, D
   Andeen, K
   Auffenberg, J
   Bai, X
   Baker, M
   Barwick, SW
   Bay, R
   Alba, JLB
   Beattie, K
   Beatty, JJ
   Bechet, S
   Becker, JK
   Becker, KH
   Benabderrahmane, ML
   BenZvi, S
   Berdermann, J
   Berghaus, P
   Berley, D
   Bernardini, E
   Bertrand, D
   Besson, DZ
   Bindig, D
   Bissok, M
   Blaufuss, E
   Blumenthal, J
   Boersma, DJ
   Bohm, C
   Bose, D
   Boser, S
   Botner, O
   Brown, AM
   Buitink, S
   Caballero-Mora, KS
   Carson, M
   Chirkin, D
   Christy, B
   Clem, J
   Clevermann, F
   Cohen, S
   Colnard, C
   Cowen, DF
   D'Agostino, MV
   Danninger, M
   Daughhetee, J
   Davis, JC
   De Clercq, C
   Demirors, L
   Denger, T
   Depaepe, O
   Descamps, F
   Desiati, P
   de Vries-Uiterweerd, G
   DeYoung, T
   Diaz-Velez, JC
   Dierckxsens, M
   Dreyer, J
   Dumm, JP
   Ehrlich, R
   Eisch, J
   Ellsworth, RW
   Engdegard, O
   Euler, S
   Evenson, PA
   Fadiran, O
   Fazely, AR
   Fedynitch, A
   Feintzeig, J
   Feusels, T
   Filimonov, K
   Finley, C
   Fischer-Wasels, T
   Foerster, MM
   Fox, BD
   Franckowiak, A
   Franke, R
   Gaisser, TK
   Gallagher, J
   Gerhardt, L
   Gladstone, L
   Glusenkamp, T
   Goldschmidt, A
   Goodman, JA
   Gora, D
   Grant, D
   Griesel, T
   Gross, A
   Grullon, S
   Gurtner, M
   Ha, C
   Hajismail, A
   Hallgren, A
   Halzen, F
   Han, K
   Hanson, K
   Heinen, D
   Helbing, K
   Herquet, P
   Hickford, S
   Hill, GC
   Hoffman, KD
   Homeier, A
   Hoshina, K
   Hubert, D
   Huelsnitz, W
   Hulss, JP
   Hulth, PO
   Hultqvist, K
   Hussain, S
   Ishihara, A
   Jacobsen, J
   Japaridze, GS
   Johansson, H
   Joseph, JM
   Kampert, KH
   Kappes, A
   Karg, T
   Karle, A
   Kenny, P
   Kiryluk, J
   Kislat, F
   Klein, SR
   Kohne, JH
   Kohnen, G
   Kolanoski, H
   Kopke, L
   Kopper, S
   Koskinen, DJ
   Kowalski, M
   Kowarik, T
   Krasberg, M
   Krings, T
   Kroll, G
   Kurahashi, N
   Kuwabara, T
   Labare, M
   Lafebre, S
   Laihem, K
   Landsman, H
   Larson, MJ
   Lauer, R
   Lunemann, J
   Madajczyk, B
   Madsen, J
   Majumdar, P
   Marotta, A
   Maruyama, R
   Mase, K
   Matis, HS
   Meagher, K
   Merck, M
   Meszaros, P
   Meures, T
   Middell, E
   Milke, N
   Miller, J
   Montaruli, T
   Morse, R
   Movit, SM
   Nahnhauer, R
   Nam, JW
   Naumann, U
   Niessen, P
   Nygren, DR
   Odrowski, S
   Olivas, A
   Olivo, M
   O'Murchadha, A
   Ono, M
   Panknin, S
   Paul, L
   de los Heros, CP
   Petrovic, J
   Piegsa, A
   Pieloth, D
   Porrata, R
   Posselt, J
   Price, CC
   Price, PB
   Przybylski, GT
   Rawlins, K
   Redl, P
   Resconi, E
   Rhode, W
   Ribordy, M
   Rizzo, A
   Rodrigues, JP
   Roth, P
   Rothmaier, F
   Rott, C
   Ruhe, T
   Rutledge, D
   Ruzybayev, B
   Ryckbosch, D
   Sander, HG
   Santander, M
   Sarkar, S
   Schatto, K
   Schmidt, T
   Schonwald, A
   Schukraft, A
   Schultes, A
   Schulz, O
   Schunck, M
   Seckel, D
   Semburg, B
   Seo, SH
   Sestayo, Y
   Seunarine, S
   Silvestri, A
   Slipak, A
   Spiczak, GM
   Spiering, C
   Stamatikos, M
   Stanev, T
   Stephens, G
   Stezelberger, T
   Stokstad, RG
   Stossl, A
   Stoyanov, S
   Strahler, EA
   Straszheim, T
   Stur, M
   Sullivan, GW
   Swillens, Q
   Taavola, H
   Taboada, I
   Tamburro, A
   Tepe, A
   Ter-Antonyan, S
   Tilav, S
   Toale, PA
   Toscano, S
   Tosi, D
   Turcan, D
   van Eijndhoven, N
   Vandenbroucke, J
   Van Overloop, A
   van Santen, J
   Vehring, M
   Voge, M
   Walck, C
   Waldenmaier, T
   Wallraff, M
   Walter, M
   Weaver, C
   Wendt, C
   Westerhoff, S
   Whitehorn, N
   Wiebe, K
   Wiebusch, CH
   Williams, DR
   Wischnewski, R
   Wissing, H
   Wolf, M
   Wood, TR
   Woschnagg, K
   Xu, C
   Xu, XW
   Yodh, G
   Yoshida, S
   Zarzhitsky, P
   Zoll, M
AF Abbasi, R.
   Abdou, Y.
   Abu-Zayyad, T.
   Adams, J.
   Aguilar, J. A.
   Ahlers, M.
   Altmann, D.
   Andeen, K.
   Auffenberg, J.
   Bai, X.
   Baker, M.
   Barwick, S. W.
   Bay, R.
   Alba, J. L. Bazo
   Beattie, K.
   Beatty, J. J.
   Bechet, S.
   Becker, J. K.
   Becker, K. -H.
   Benabderrahmane, M. L.
   BenZvi, S.
   Berdermann, J.
   Berghaus, P.
   Berley, D.
   Bernardini, E.
   Bertrand, D.
   Besson, D. Z.
   Bindig, D.
   Bissok, M.
   Blaufuss, E.
   Blumenthal, J.
   Boersma, D. J.
   Bohm, C.
   Bose, D.
   Boeser, S.
   Botner, O.
   Brown, A. M.
   Buitink, S.
   Caballero-Mora, K. S.
   Carson, M.
   Chirkin, D.
   Christy, B.
   Clem, J.
   Clevermann, F.
   Cohen, S.
   Colnard, C.
   Cowen, D. F.
   D'Agostino, M. V.
   Danninger, M.
   Daughhetee, J.
   Davis, J. C.
   De Clercq, C.
   Demiroers, L.
   Denger, T.
   Depaepe, O.
   Descamps, F.
   Desiati, P.
   de Vries-Uiterweerd, G.
   DeYoung, T.
   Diaz-Velez, J. C.
   Dierckxsens, M.
   Dreyer, J.
   Dumm, J. P.
   Ehrlich, R.
   Eisch, J.
   Ellsworth, R. W.
   Engdegard, O.
   Euler, S.
   Evenson, P. A.
   Fadiran, O.
   Fazely, A. R.
   Fedynitch, A.
   Feintzeig, J.
   Feusels, T.
   Filimonov, K.
   Finley, C.
   Fischer-Wasels, T.
   Foerster, M. M.
   Fox, B. D.
   Franckowiak, A.
   Franke, R.
   Gaisser, T. K.
   Gallagher, J.
   Gerhardt, L.
   Gladstone, L.
   Gluesenkamp, T.
   Goldschmidt, A.
   Goodman, J. A.
   Gora, D.
   Grant, D.
   Griesel, T.
   Gross, A.
   Grullon, S.
   Gurtner, M.
   Ha, C.
   Hajismail, A.
   Hallgren, A.
   Halzen, F.
   Han, K.
   Hanson, K.
   Heinen, D.
   Helbing, K.
   Herquet, P.
   Hickford, S.
   Hill, G. C.
   Hoffman, K. D.
   Homeier, A.
   Hoshina, K.
   Hubert, D.
   Huelsnitz, W.
   Huelss, J. -P.
   Hulth, P. O.
   Hultqvist, K.
   Hussain, S.
   Ishihara, A.
   Jacobsen, J.
   Japaridze, G. S.
   Johansson, H.
   Joseph, J. M.
   Kampert, K. -H.
   Kappes, A.
   Karg, T.
   Karle, A.
   Kenny, P.
   Kiryluk, J.
   Kislat, F.
   Klein, S. R.
   Koehne, J. -H.
   Kohnen, G.
   Kolanoski, H.
   Koepke, L.
   Kopper, S.
   Koskinen, D. J.
   Kowalski, M.
   Kowarik, T.
   Krasberg, M.
   Krings, T.
   Kroll, G.
   Kurahashi, N.
   Kuwabara, T.
   Labare, M.
   Lafebre, S.
   Laihem, K.
   Landsman, H.
   Larson, M. J.
   Lauer, R.
   Luenemann, J.
   Madajczyk, B.
   Madsen, J.
   Majumdar, P.
   Marotta, A.
   Maruyama, R.
   Mase, K.
   Matis, H. S.
   Meagher, K.
   Merck, M.
   Meszaros, P.
   Meures, T.
   Middell, E.
   Milke, N.
   Miller, J.
   Montaruli, T.
   Morse, R.
   Movit, S. M.
   Nahnhauer, R.
   Nam, J. W.
   Naumann, U.
   Niessen, P.
   Nygren, D. R.
   Odrowski, S.
   Olivas, A.
   Olivo, M.
   O'Murchadha, A.
   Ono, M.
   Panknin, S.
   Paul, L.
   de los Heros, C. Perez
   Petrovic, J.
   Piegsa, A.
   Pieloth, D.
   Porrata, R.
   Posselt, J.
   Price, C. C.
   Price, P. B.
   Przybylski, G. T.
   Rawlins, K.
   Redl, P.
   Resconi, E.
   Rhode, W.
   Ribordy, M.
   Rizzo, A.
   Rodrigues, J. P.
   Roth, P.
   Rothmaier, F.
   Rott, C.
   Ruhe, T.
   Rutledge, D.
   Ruzybayev, B.
   Ryckbosch, D.
   Sander, H. -G.
   Santander, M.
   Sarkar, S.
   Schatto, K.
   Schmidt, T.
   Schoenwald, A.
   Schukraft, A.
   Schultes, A.
   Schulz, O.
   Schunck, M.
   Seckel, D.
   Semburg, B.
   Seo, S. H.
   Sestayo, Y.
   Seunarine, S.
   Silvestri, A.
   Slipak, A.
   Spiczak, G. M.
   Spiering, C.
   Stamatikos, M.
   Stanev, T.
   Stephens, G.
   Stezelberger, T.
   Stokstad, R. G.
   Stoessl, A.
   Stoyanov, S.
   Strahler, E. A.
   Straszheim, T.
   Stuer, M.
   Sullivan, G. W.
   Swillens, Q.
   Taavola, H.
   Taboada, I.
   Tamburro, A.
   Tepe, A.
   Ter-Antonyan, S.
   Tilav, S.
   Toale, P. A.
   Toscano, S.
   Tosi, D.
   Turcan, D.
   van Eijndhoven, N.
   Vandenbroucke, J.
   Van Overloop, A.
   van Santen, J.
   Vehring, M.
   Voge, M.
   Walck, C.
   Waldenmaier, T.
   Wallraff, M.
   Walter, M.
   Weaver, Ch.
   Wendt, C.
   Westerhoff, S.
   Whitehorn, N.
   Wiebe, K.
   Wiebusch, C. H.
   Williams, D. R.
   Wischnewski, R.
   Wissing, H.
   Wolf, M.
   Wood, T. R.
   Woschnagg, K.
   Xu, C.
   Xu, X. W.
   Yodh, G.
   Yoshida, S.
   Zarzhitsky, P.
   Zoll, M.
CA IceCube Collaboration
TI OBSERVATION OF ANISOTROPY IN THE ARRIVAL DIRECTIONS OF GALACTIC COSMIC
   RAYS AT MULTIPLE ANGULAR SCALES WITH IceCube
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; cosmic rays
ID MILAGRO HOT-SPOTS; AIR-SHOWER ARRAY; ENERGY-SPECTRUM; INTENSITY;
   TELESCOPE; ASTRONOMY
AB Between 2009 May and 2010 May, the IceCube neutrino detector at the South Pole recorded 32 billion muons generated in air showers produced by cosmic rays with a median energy of 20 TeV. With a data set of this size, it is possible to probe the southern sky for per-mil anisotropy on all angular scales in the arrival direction distribution of cosmic rays. Applying a power spectrum analysis to the relative intensity map of the cosmic ray flux in the southern hemisphere, we show that the arrival direction distribution is not isotropic, but shows significant structure on several angular scales. In addition to previously reported large-scale structure in the form of a strong dipole and quadrupole, the data show small-scale structure on scales between 15 degrees and 30 degrees. The skymap exhibits several localized regions of significant excess and deficit in cosmic ray intensity. The relative intensity of the smaller-scale structures is about a factor of five weaker than that of the dipole and quadrupole structure. The most significant structure, an excess localized at (right ascension alpha = 122 degrees.4 and declination d = -47 degrees.4), extends over at least 20 degrees in right ascension and has a post-trials significance of 5.3 sigma. The origin of this anisotropy is still unknown.
C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Madajczyk, B.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Price, C. C.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
   [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Hajismail, A.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
   [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
   [Adams, J.; Brown, A. M.; Gross, A.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
   [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
   [Altmann, D.; Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Gluesenkamp, T.; Heinen, D.; Huelss, J. -P.; Krings, T.; Laihem, K.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
   [Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
   [Bai, X.; Berghaus, P.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
   [Bai, X.; Berghaus, P.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
   [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Gora, D.; Han, K.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
   [Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
   [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
   [Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle, Columbus, OH 43210 USA.
   [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
   [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Meures, T.; Petrovic, J.; Swillens, Q.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium.
   [Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
   [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
   [Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
   [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
   [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
   [Bose, D.; Buitink, S.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
   [Boeser, S.; Denger, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Stuer, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
   [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
   [Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Rutledge, D.; Slipak, A.; Stephens, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
   [Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
   [Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
   [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
   [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
   [Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
   [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
   [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
   [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
   [Grant, D.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
   [Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
   [Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
   [Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
   [Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
   [Montaruli, T.] Univ Bari, Dipartmento Fis, I-70126 Bari, Italy.
   [Montaruli, T.] Sezione Ist Nazl Fis Nucl, Bari, Italy.
   [Rawlins, K.] Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA.
   [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
   [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Toale, P. A.; Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
RI Wiebusch, Christopher/G-6490-2012; Tamburro, Alessio/A-5703-2013;
   Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Tjus,
   Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014; Koskinen,
   David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama,
   Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011;
   Taavola, Henric/B-4497-2011; 
OI Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg,
   Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar
   Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama,
   Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty,
   James/0000-0003-0481-4952; Ter-Antonyan, Samvel/0000-0002-5788-1369;
   Schukraft, Anne/0000-0002-9112-5479; Perez de los Heros,
   Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810;
   Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819;
   Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed
   Lotfi/0000-0003-4410-5886
FU U. S National Science Foundation-Office of Polar Programs; U. S National
   Science Foundation-Physics Division; University of Wisconsin Alumni
   Research Foundation; Grid Laboratory Of Wisconsin (GLOW) at the
   University of Wisconsin-Madison; Open Science Grid (OSG) grid
   infrastructure; U. S Department of Energy; National Energy Research
   Scientific Computing Center; Louisiana Optical Network Initiative (LONI)
   grid computing resources; National Science and Engineering Research
   Council of Canada; Swedish Research Council; Swedish Polar Research
   Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut
   and Alice Wallenberg Foundation, Sweden; German Ministry for Education
   and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research
   Department of Plasmas with Complex Interactions (Bochum), Germany; Fund
   for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders
   Institute to encourage scientific and technological research in industry
   (IWT); Belgian Federal Science Policy Office (Belspo); University of
   Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for
   Promotion of Science (JSPS); Swiss National Science Foundation (SNSF),
   Switzerland; EU; Capes Foundation, Ministry of Education of Brazi
FX We acknowledge the support from the following agencies: U. S National
   Science Foundation-Office of Polar Programs, U. S National Science
   Foundation-Physics Division, University of Wisconsin Alumni Research
   Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
   at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
   infrastructure; U. S Department of E nergy, and National Energy Research
   Scientific Computing Center, the Louisiana Optical Network Initiative
   (LONI) grid computing resources; National Science and Engineering
   Research Council of Canada; Swedish Research Council, Swedish Polar
   Research Secretariat, Swedish National Infrastructure for Computing
   (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German
   Ministry for Education and Research (BMBF), Deutsche
   Forschungsgemeinschaft (DFG), Research Department of Plasmas with
   Complex Interactions (Bochum), Germany; Fund for Scientific Research
   (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage
   scientific and technological research in industry (IWT), Belgian Federal
   Science Policy Office (Belspo); University of Oxford, United Kingdom;
   Marsden Fund, New Zealand; Japan Society for Promotion of Science
   (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A.
   Gross acknowledges support by the EU Marie Curie OIF Program; J. P.
   Rodrigues acknowledges support by the Capes Foundation, Ministry of
   Education of Brazil.
NR 37
TC 58
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
AR 16
DI 10.1088/0004-637X/740/1/16
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825FL
UT WOS:000295256500016
ER

PT J
AU Deming, D
   Sada, PV
   Jackson, B
   Peterson, SW
   Agol, E
   Knutson, HA
   Jennings, DE
   Haase, F
   Bays, K
AF Deming, Drake
   Sada, Pedro V.
   Jackson, Brian
   Peterson, Steven W.
   Agol, Eric
   Knutson, Heather A.
   Jennings, Donald E.
   Haase, Flynn
   Bays, Kevin
TI KEPLER AND GROUND-BASED TRANSITS OF THE EXO-NEPTUNE HAT-P-11b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: general; stars: activity;
   starspots
ID LIMB-DARKENING COEFFICIENTS; EXOPLANET GJ 1214B; EXTRASOLAR PLANET;
   SUPER-EARTH; LIGHT-CURVE; THERMAL EMISSION; STAR; ORBIT; FIELD; MASS
AB We analyze 26 archival Kepler transits of the exo-Neptune HAT-P-11b, supplemented by ground-based transits observed in the blue (B band) and near-IR (J band). Both the planet and host star are smaller than previously believed; our analysis yields R-p = 4.31 R-circle plus +/- 0.06R(circle plus) and R-s = 0.683R(circle dot) +/- 0.009R(circle dot), both about 3 sigma smaller than the discovery values. Our ground-based transit data at wavelengths bracketing the Kepler bandpass serve to check the wavelength dependence of stellar limb darkening, and the J-band transit provides a precise and independent constraint on the transit duration. Both the limb darkening and transit duration from our ground-based data are consistent with the new Kepler values for the system parameters. Our smaller radius for the planet implies that its gaseous envelope can be less extensive than previously believed, being very similar to the H-He envelope of GJ 436b and Kepler-4b. HAT-P-11 is an active star, and signatures of star spot crossings are ubiquitous in the Kepler transit data. We develop and apply a methodology to correct the planetary radius for the presence of both crossed and uncrossed star spots. Star spot crossings are concentrated at phases -0.002 and +0.006. This is consistent with inferences from Rossiter-McLaughlin measurements that the planet transits nearly perpendicular to the stellar equator. We identify the dominant phases of star spot crossings with active latitudes on the star, and infer that the stellar rotational pole is inclined at about 12 degrees +/- 5 degrees to the plane of the sky. We point out that precise transit measurements over long durations could in principle allow us to construct a stellar Butterfly diagram to probe the cyclic evolution of magnetic activity on this active K-dwarf star.
C1 [Deming, Drake; Jackson, Brian; Jennings, Donald E.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
   [Sada, Pedro V.] Univ Monterrey, Dept Fis & Matemat, Monterrey, Mexico.
   [Peterson, Steven W.; Haase, Flynn; Bays, Kevin] Natl Opt Astron Observ, Kitt Peak Natl Observ, Tucson, AZ 85719 USA.
   [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
   [Agol, Eric; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Deming, D (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM ddeming@astro.umd.edu
RI Jennings, Donald/D-7978-2012; Agol, Eric/B-8775-2013
OI Agol, Eric/0000-0002-0802-9145
FU NSF [AST-0645416]
FX We thank Dick Joyce for his expert assistance with FLAMINGOS, and we
   thank the anonymous referee for insightful comments that allowed us to
   improve this paper. Eric Agol acknowledges support from NSF Career grant
   AST-0645416.
NR 36
TC 31
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
AR 33
DI 10.1088/0004-637X/740/1/33
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825FL
UT WOS:000295256500033
ER

PT J
AU Kataoka, J
   Stawarz, L
   Takahashi, Y
   Cheung, CC
   Hayashida, M
   Grandi, P
   Burnett, TH
   Celotti, A
   Fegan, SJ
   Fortin, P
   Maeda, K
   Nakamori, T
   Taylor, GB
   Tosti, G
   Digel, SW
   McConville, W
   Finke, J
   D'Ammando, F
AF Kataoka, J.
   Stawarz, L.
   Takahashi, Y.
   Cheung, C. C.
   Hayashida, M.
   Grandi, P.
   Burnett, T. H.
   Celotti, A.
   Fegan, S. J.
   Fortin, P.
   Maeda, K.
   Nakamori, T.
   Taylor, G. B.
   Tosti, G.
   Digel, S. W.
   McConville, W.
   Finke, J.
   D'Ammando, F.
TI BROAD-LINE RADIO GALAXIES OBSERVED WITH FERMI-LAT: THE ORIGIN OF THE GeV
   gamma-RAY EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (3C 120, 3C 111); galaxies: jets;
   gamma rays: galaxies; radiation mechanisms: non-thermal; X-rays:
   galaxies
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; ADVECTION-DOMINATED
   ACCRETION; BLACK-HOLE MASS; XMM-NEWTON OBSERVATION; BRIGHT QUASAR
   SURVEY; ALL-SKY SURVEY; X-RAY; VLBI OBSERVATIONS; COMPLETE SAMPLE
AB We report on a detailed investigation of the gamma-ray emission from 18 broad-line radio galaxies (BLRGs) based on two years of Fermi Large Area Telescope data. We confirm the previously reported detections of 3C 120 and 3C 111 in the GeV photon energy range; a detailed look at the temporal characteristics of the observed gamma-ray emission reveals in addition possible flux variability in both sources. No statistically significant gamma-ray detection of the other BLRGs was found, however, in the considered data set. Though the sample size studied is small, what appears to differentiate 3C 111 and 3C 120 from the BLRGs not yet detected in gamma-rays is the particularly strong nuclear radio flux. This finding, together with the indications of the gamma-ray flux variability and a number of other arguments presented, indicates that the GeV emission of BLRGs is most likely dominated by the beamed radiation of relativistic jets observed at intermediate viewing angles. In this paper we also analyzed a comparison sample of high-accretion-rate Seyfert 1 galaxies, which can be considered radio-quiet counterparts of BLRGs, and found that none were detected in gamma-rays. A simple phenomenological hybrid model applied for the broadband emission of the discussed radio-loud and radio-quiet type 1 active galaxies suggests that the relative contribution of the nuclear jets to the accreting matter is >= 1% on average for BLRGs, whereas it is <= 0.1% for Seyfert 1 galaxies.
C1 [Kataoka, J.; Takahashi, Y.; Maeda, K.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Tokyo 1698555, Japan.
   [Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Kanagawa 2525210, Japan.
   [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
   [Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA.
   [Hayashida, M.; Digel, S. W.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
   [Grandi, P.] INAF IASF Bologna, I-40129 Bologna, Italy.
   [Hayashida, M.; Digel, S. W.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
   [Burnett, T. H.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
   [Celotti, A.] SISSA, I-34014 Trieste, Italy.
   [Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France.
   [Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
   [Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
   [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
   [McConville, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [McConville, W.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
   [McConville, W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Finke, J.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
   [D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy.
   [D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
RP Kataoka, J (reprint author), Waseda Univ, Res Inst Sci & Engn, Tokyo 1698555, Japan.
EM kataoka.jun@waseda.jp
RI Tosti, Gino/E-9976-2013; 
OI Grandi, Paola/0000-0003-1848-6013
FU National Aeronautics and Space Administration; Department of Energy in
   the United States; Commissariat a l'EnergieAtomique; Centre National de
   la Recherche Scientifique/Institut National de Physique Nucleaire et de
   Physique des Particules in France; Agenzia Spaziale Italiana; Istituto
   Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture,
   Sports, Science and Technology (MEXT); High Energy Accelerator Research
   Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan;
   K. A. Wallenberg Foundation; Swedish Research Council; Swedish National
   Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy;
   Centre National d'Etudes Spatiales in France; University of Michigan;
   National Science Foundation [AST-0607523]; Polish MNiSW [N-N203-380336]
FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a
   number of agencies and institutes that have supported both the
   development and the operation of the LAT as well as scientific data
   analysis. These include the National Aeronautics and Space
   Administration and the Department of Energy in the United States, the
   Commissariat a l'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.;
   Additional support for science analysis during the operations phase is
   gratefully acknowledged from the Istituto Nazionale di Astrofisica in
   Italy and the Centre National d'Etudes Spatiales in France.; This
   research has made use of data from the University of Michigan Radio
   Astronomy Observatory, which has been supported by the University of
   Michigan and by a series of grants from the National Science Foundation,
   most recently AST-0607523.; L.S. acknowledges the support from the
   Polish MNiSW through the grant N-N203-380336. We thank the anonymous
   referee for critical comments which helped to improve the paper.
NR 140
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
AR 29
DI 10.1088/0004-637X/740/1/29
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825FL
UT WOS:000295256500029
ER

PT J
AU Luo, B
   Brandt, WN
   Xue, YQ
   Alexander, DM
   Brusa, M
   Bauer, FE
   Comastri, A
   Fabian, AC
   Gilli, R
   Lehmer, BD
   Rafferty, DA
   Schneider, DP
   Vignali, C
AF Luo, B.
   Brandt, W. N.
   Xue, Y. Q.
   Alexander, D. M.
   Brusa, M.
   Bauer, F. E.
   Comastri, A.
   Fabian, A. C.
   Gilli, R.
   Lehmer, B. D.
   Rafferty, D. A.
   Schneider, D. P.
   Vignali, C.
TI REVEALING A POPULATION OF HEAVILY OBSCURED ACTIVE GALACTIC NUCLEI AT z
   approximate to 0.5-1 IN THE CHANDRA DEEP FIELD-SOUTH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; galaxies: active; galaxies: photometry;
   galaxies: starburst; infrared: galaxies; X-rays: galaxies
ID STAR-FORMATION RATE; ULTRALUMINOUS INFRARED GALAXIES; COMPTON-THICK AGN;
   X-RAY-EMISSION; POINT-SOURCE CATALOGS; MS SOURCE CATALOGS; PHOTOMETRIC
   REDSHIFTS; FORMING GALAXIES; NEARBY GALAXIES; STELLAR-MASS
AB Heavily obscured (NH greater than or similar to 3 x 10(23) cm(-2)) active galactic nuclei (AGNs) not detected even in the deepest X-ray surveys are often considered to be comparably numerous to the unobscured and moderately obscured AGNs. Such sources are required to fit the cosmic X-ray background (XRB) emission in the 10-30 keV band. We identify a numerically significant population of heavily obscured AGNs at z approximate to 0.5-1 in the Chandra Deep Field-South (CDF-S) and Extended Chandra Deep Field-South by selecting 242 X-ray undetected objects with infrared-based star-formation rates (SFRs) substantially higher (a factor of 3.2 or more) than their SFRs determined from the UV after correcting for dust extinction. An X-ray stacking analysis of 23 candidates in the central CDF-S region using the 4 Ms Chandra data reveals a hard X-ray signal with an effective power-law photon index of Gamma = 0.6(-0.4)(+ 0.3), indicating a significant contribution from obscured AGNs. Based on Monte Carlo simulations, we conclude that 74% +/- 25% of the selected galaxies host obscured AGNs, within which approximate to 95% are heavily obscured and approximate to 80% are Compton-thick (CT; N-H > 1.5 x 10(24) cm(-2)). The heavily obscured objects in our sample are of moderate intrinsic X-ray luminosity (approximate to(0.9-4) x 10(42) erg s(-1) in the 2-10 keV band). The space density of the CT AGNs is (1.6 +/- 0.5) x 10(-4) Mpc(-3). The z approximate to 0.5-1 CT objects studied here are expected to contribute approximate to 1% of the total XRB flux in the 10-30 keV band, and they account for approximate to 5%-15% of the emission in this energy band expected from all CT AGNs according to population-synthesis models. In the 6-8 keV band, the stacked signal of the 23 heavily obscured candidates accounts for <5% of the unresolved XRB flux, while the unresolved approximate to 25% of the XRB in this band can probably be explained by a stacking analysis of the X-ray undetected optical galaxies in the CDF-S (a 2.5 sigma stacked signal). We discuss prospects to identify such heavily obscured objects using future hard X-ray observatories.
C1 [Luo, B.; Brandt, W. N.; Xue, Y. Q.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Luo, B.; Brandt, W. N.; Xue, Y. Q.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
   [Luo, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
   [Brusa, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
   [Comastri, A.; Gilli, R.] INAF Osservatorio Astron Bologna, Bologna, Italy.
   [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Lehmer, B. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
   [Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Rafferty, D. A.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
   [Vignali, C.] Univ Bologna, Dipartimento Astron, Bologna, Italy.
RP Luo, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Comastri,
   Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; 
OI Vignali, Cristian/0000-0002-8853-9611; Brandt,
   William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970;
   Gilli, Roberto/0000-0001-8121-6177; Alexander, David/0000-0002-5896-6313
FU CXC [SP1-12007A, G09-0134A]; NASA [NNX10AC99G]; Science and Technology
   Facilities Council; ASI/INAF [I/009/10/0]
FX We acknowledge financial support from CXC grant SP1-12007A (B.L.,
   W.N.B., Y.Q.X.), CXC grant G09-0134A (B. L., W.N.B., Y.Q.X.), NASA ADP
   grant NNX10AC99G (W.N.B.), the Science and Technology Facilities Council
   (D.M.A.), and ASI/INAF grant I/009/10/0 (A.C., C.V., R.G.). We are
   grateful to T. Yaqoob and K. D. Murphy for providing support for the
   MYTORUS model and making available the data for our desired half-opening
   angle. We thank A. T. Steffen for helpful discussions. We also thank the
   referee for carefully reviewing the manuscript and providing helpful
   comments that improved this work.
NR 126
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
AR 37
DI 10.1088/0004-637X/740/1/37
PG 15
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SC Astronomy & Astrophysics
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ER

PT J
AU Reiter, M
   Shirley, YL
   Wu, JW
   Brogan, C
   Wootten, A
   Tatematsu, K
AF Reiter, Megan
   Shirley, Yancy L.
   Wu, Jingwen
   Brogan, Crystal
   Wootten, Alwyn
   Tatematsu, Ken'ichi
TI EVIDENCE FOR INFLOW IN HIGH-MASS STAR-FORMING CLUMPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; stars: formation
ID YOUNG STELLAR OBJECTS; IRAS 16293-2422; MOLECULAR CLOUDS; PROPER
   MOTIONS; CLASS-I; INFALL; OUTFLOWS; REGIONS; CORES; HCO+
AB We analyze the HCO+ 3-2 and (HCO+)-C-13 3-2 line profiles of 27 high-mass star-forming regions to identify asymmetries that are suggestive of mass inflow. Three quantitative measures of line asymmetry are used to indicate whether a line profile is blue, red, or neither-the ratio of the temperature of the blue and red peaks, the line skew, and the dimensionless parameter delta upsilon. We find nine HCO+ 3-2 line profiles with a significant blue asymmetry and four with significant red asymmetric profiles. Comparing our HCO+ 3-2 results to HCN 3-2 observations from Wu et al., we find that eight of the blue and three of the red have profiles with the same asymmetry in HCN. The eight sources with blue asymmetries in both tracers are considered strong candidates for inflow. Quantitative measures of the asymmetry (e.g., delta upsilon) tend to be larger for HCN. This, combined with possible HCO+ abundance enhancements in outflows, suggests that HCN may be a better tracer of inflow. Understanding the behavior of common molecular tracers like HCO+ in clumps of different masses is important for properly analyzing the line profiles seen in a sample of sources representing a broad range of clump masses. Such studies will soon be possible with the large number of sources with possible self-absorption seen in spectroscopic follow-up observations of clumps identified in the Bolocam Galactic Plane Survey.
C1 [Reiter, Megan; Shirley, Yancy L.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
   [Wu, Jingwen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Brogan, Crystal; Wootten, Alwyn] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
   [Tatematsu, Ken'ichi] Natl Astron Observ Japan, Mitaka Tokyo 1818588, Japan.
RP Reiter, M (reprint author), Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA.
EM mreiter@as.arizona.edu; yshirley@as.arizona.edu;
   jingwen.wu@jpl.nasa.gov; cbrogan@nrao.edu; awootten@nrao.edu;
   k.tatematsu@nao.ac.jp
FU NSF [AST-1008577]
FX We thank Wayne Schlingman and Patrick Fimbres for their assistance with
   the HHT observations. Yancy Shirley is partially supported by NSF grant
   AST-1008577.
NR 40
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
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DI 10.1088/0004-637X/740/1/40
PG 6
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SC Astronomy & Astrophysics
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UT WOS:000295256500040
ER

PT J
AU Serra, P
   Amblard, A
   Temi, P
   Burgarella, D
   Giovannoli, E
   Buat, V
   Noll, S
   Im, S
AF Serra, Paolo
   Amblard, Alexandre
   Temi, Pasquale
   Burgarella, Denis
   Giovannoli, Elodie
   Buat, Veronique
   Noll, Stefan
   Im, Stephen
TI CIGALEMC: GALAXY PARAMETER ESTIMATION USING A MARKOV CHAIN MONTE CARLO
   APPROACH WITH CIGALE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: fundamental parameters; methods: data analysis
ID STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; STELLAR POPULATION
   SYNTHESIS; NEARBY GALAXIES; INFRARED-EMISSION; STARBURST GALAXIES;
   EXTINCTION CURVES; INTERSTELLAR DUST; ULTRAVIOLET; EVOLUTION
AB We introduce a fast Markov Chain Monte Carlo (MCMC) exploration of the astrophysical parameter space using a modified version of the publicly available code Code Investigating GALaxy Emission (CIGALE). The original CIGALE builds a grid of theoretical spectral energy distribution (SED) models and fits to photometric fluxes from ultraviolet to infrared to put constraints on parameters related to both formation and evolution of galaxies. Such a grid-based method can lead to a long and challenging parameter extraction since the computation time increases exponentially with the number of parameters considered and results can be dependent on the density of sampling points, which must be chosen in advance for each parameter. MCMC methods, on the other hand, scale approximately linearly with the number of parameters, allowing a faster and more accurate exploration of the parameter space by using a smaller number of efficiently chosen samples. We test our MCMC version of the code CIGALE (called CIGALEMC) with simulated data. After checking the ability of the code to retrieve the input parameters used to build the mock sample, we fit theoretical SEDs to real data from the well-known and -studied Spitzer Infrared Nearby Galaxy Survey sample. We discuss constraints on the parameters and show the advantages of our MCMC sampling method in terms of accuracy of the results and optimization of CPU time.
C1 [Serra, Paolo; Amblard, Alexandre; Temi, Pasquale; Im, Stephen] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
   [Burgarella, Denis; Giovannoli, Elodie; Buat, Veronique] Observ Astron Marseille Provence, F-13388 Marseille 13, France.
   [Noll, Stefan] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
RP Serra, P (reprint author), NASA, Ames Res Ctr, Astrophys Branch, MS 245-6, Moffett Field, CA 94035 USA.
RI Serra, Paolo/G-9678-2014; amblard, alexandre/L-7694-2014
OI Serra, Paolo/0000-0002-7609-3931; amblard, alexandre/0000-0002-2212-5395
NR 48
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
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DI 10.1088/0004-637X/740/1/22
PG 11
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SC Astronomy & Astrophysics
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UT WOS:000295256500022
ER

PT J
AU Skemer, AJ
   Close, LM
   Greene, TP
   Hinz, PM
   Hoffmann, WF
   Males, JR
AF Skemer, Andrew J.
   Close, Laird M.
   Greene, Thomas P.
   Hinz, Philip M.
   Hoffmann, William F.
   Males, Jared R.
TI DUST GRAIN EVOLUTION IN SPATIALLY RESOLVED T TAURI BINARIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; instrumentation: adaptive optics; planets and
   satellites: formation; protoplanetary disks; stars: variables: T Tauri,
   Herbig Ae/Be
ID STAR-FORMING REGIONS; SPITZER-IRS SPECTRA; LOW-MASS STARS; AURIGA
   MOLECULAR CLOUD; HUBBLE-SPACE-TELESCOPE; ADAPTIVE OPTICS SYSTEM; BROWN
   DWARF DISKS; PROTOPLANETARY DISKS; CRYSTALLINE SILICATES; SPECTROSCOPIC
   SURVEY
AB Core-accretion planet formation begins in protoplanetary disks with the growth of small, interstellar medium dust grains into larger particles. The progress of grain growth, which can be quantified using 10 mu m silicate spectroscopy, has broad implications for the final products of planet formation. Previous studies have attempted to correlate stellar and disk properties with the 10 mu m silicate feature in an effort to determine which stars are efficient at grain growth. Thus far there does not appear to be a dominant correlated parameter. In this paper, we use spatially resolved adaptive optics spectroscopy of nine T Tauri binaries as tight as 0 ''.25 to determine if basic properties shared between binary stars, such as age, composition, and formation history, have an effect on dust grain evolution. We find with 90%-95% confidence that the silicate feature equivalent widths of binaries are more similar than those of randomly paired single stars, implying that shared properties do play an important role in dust grain evolution. At lower statistical significance, we find with 82% confidence that the secondary has a more prominent silicate emission feature (i.e., smaller grains) than the primary. If confirmed by larger surveys, this would imply that spectral type and/or binarity are important factors in dust grain evolution.
C1 [Skemer, Andrew J.; Close, Laird M.; Hinz, Philip M.; Hoffmann, William F.; Males, Jared R.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA.
   [Greene, Thomas P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Skemer, AJ (reprint author), Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA.
OI Skemer, Andrew/0000-0001-6098-3924
FU NSF
FX The authors thank Elise Furlan, Mitsuhiko Honda, and Dan Watson for
   providing their published spectra. We also thank Daniel Apai, Ilaria
   Pascucci, and Kevin Flaherty for useful discussions regarding grain
   growth and silicate variability. A.J.S. acknowledges the NASA Graduate
   Student Research Program (GSRP) for its generous support of this
   project. L.M.C. thanks the NSF AAG Program for support of this research.
   We also thank the MMT staff, especially Mike Alegria, Morag Hastie, and
   Ricardo Ortiz for operating the AO system during a difficult set of
   observations.
NR 78
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
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DI 10.1088/0004-637X/740/1/43
PG 14
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SC Astronomy & Astrophysics
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UT WOS:000295256500043
ER

PT J
AU Winebarger, AR
   Schmelz, JT
   Warren, HP
   Saar, SH
   Kashyap, VL
AF Winebarger, Amy R.
   Schmelz, Joan T.
   Warren, Harry P.
   Saar, Steve H.
   Kashyap, Vinay L.
TI USING A DIFFERENTIAL EMISSION MEASURE AND DENSITY MEASUREMENTS IN AN
   ACTIVE REGION CORE TO TEST A STEADY HEATING MODEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona
ID X-RAY TELESCOPE; ULTRAVIOLET IMAGING SPECTROMETER; SOLAR-B SATELLITE;
   CORONAL LOOPS; TEMPERATURE DISTRIBUTION; SOHO EIT; HINODE; MOSS; TRACE;
   MISSION
AB The frequency of heating events in the corona is an important constraint on the coronal heating mechanisms. Observations indicate that the intensities and velocities measured in active region cores are effectively steady, suggesting that heating events occur rapidly enough to keep high-temperature active region loops close to equilibrium. In this paper, we couple observations of active region (AR) 10955 made with the X-Ray Telescope and the EUV Imaging Spectrometer on board Hinode to test a simple steady heating model. First we calculate the differential emission measure (DEM) of the apex region of the loops in the active region core. We find the DEM to be broad and peaked around 3 MK. We then determine the densities in the corresponding footpoint regions. Using potential field extrapolations to approximate the loop lengths and the density-sensitive line ratios to infer the magnitude of the heating, we build a steady heating model for the active region core and find that we can match the general properties of the observed DEM for the temperature range of 6.3 < log T < 6.7. This model, for the first time, accounts for the base pressure, loop length, and distribution of apex temperatures of the core loops. We find that the density-sensitive spectral line intensities and the bulk of the hot emission in the active region core are consistent with steady heating. We also find, however, that the steady heating model cannot address the emission observed at lower temperatures. This emission may be due to foreground or background structures, or may indicate that the heating in the core is more complicated. Different heating scenarios must be tested to determine if they have the same level of agreement.
C1 [Winebarger, Amy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Schmelz, Joan T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
   [Warren, Harry P.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
   [Saar, Steve H.; Kashyap, Vinay L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA.
EM amy.r.winebarger@nasa.gov
FU NSF; NASA/SAO
FX A.R.W. was supported by an NSF Career grant. Solar physics research at
   the University of Memphis is supported by a Hinode subcontract from
   NASA/SAO. A. R. W. thanks Mark Weber for many enlightening conversations
   on differential emission measures.
NR 56
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
AR 2
DI 10.1088/0004-637X/740/1/2
PG 12
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SC Astronomy & Astrophysics
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UT WOS:000295256500002
ER

PT J
AU Aguirre, VS
   Chaplin, WJ
   Ballot, J
   Basu, S
   Bedding, TR
   Serenelli, AM
   Verner, GA
   Miglio, A
   Monteiro, MJPFG
   Weiss, A
   Appourchaux, T
   Bonanno, A
   Broomhall, AM
   Bruntt, H
   Campante, TL
   Casagrande, L
   Corsaro, E
   Elsworth, Y
   Garcia, RA
   Gaulme, P
   Handberg, R
   Hekker, S
   Huber, D
   Karoff, C
   Mathur, S
   Mosser, B
   Salabert, D
   Schonrich, R
   Sousa, SG
   Stello, D
   White, TR
   Christensen-Dalsgaard, J
   Gilliland, RL
   Kawaler, SD
   Kjeldsen, H
   Houdek, G
   Metcalfe, TS
   Molenda-Zakowicz, J
   Thompson, MJ
   Caldwell, DA
   Christiansen, JL
   Wohler, B
AF Aguirre, V. Silva
   Chaplin, W. J.
   Ballot, J.
   Basu, S.
   Bedding, T. R.
   Serenelli, A. M.
   Verner, G. A.
   Miglio, A.
   Monteiro, M. J. P. F. G.
   Weiss, A.
   Appourchaux, T.
   Bonanno, A.
   Broomhall, A. M.
   Bruntt, H.
   Campante, T. L.
   Casagrande, L.
   Corsaro, E.
   Elsworth, Y.
   Garcia, R. A.
   Gaulme, P.
   Handberg, R.
   Hekker, S.
   Huber, D.
   Karoff, C.
   Mathur, S.
   Mosser, B.
   Salabert, D.
   Schoenrich, R.
   Sousa, S. G.
   Stello, D.
   White, T. R.
   Christensen-Dalsgaard, J.
   Gilliland, R. L.
   Kawaler, S. D.
   Kjeldsen, H.
   Houdek, G.
   Metcalfe, T. S.
   Molenda-Zakowicz, J.
   Thompson, M. J.
   Caldwell, D. A.
   Christiansen, J. L.
   Wohler, B.
TI CONSTRUCTING A ONE-SOLAR-MASS EVOLUTIONARY SEQUENCE USING ASTEROSEISMIC
   DATA FROM KEPLER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE asteroseismology; stars: evolution; stars: oscillations
ID GLOBAL OSCILLATION PARAMETERS; RED GIANT STARS; 1ST 4 MONTHS;
   MAIN-SEQUENCE; CHEMICAL EVOLUTION; AMPLITUDES; PROGRAM; MISSION; RADIUS;
   COROT
AB Asteroseismology of solar-type stars has entered a new era of large surveys with the success of the NASA Kepler mission, which is providing exquisite data on oscillations of stars across the Hertzsprung-Russell diagram. From the time-series photometry, the two seismic parameters that can be most readily extracted are the large frequency separation (Delta nu) and the frequency of maximum oscillation power (nu(max)). After the survey phase, these quantities are available for hundreds of solar-type stars. By scaling from solar values, we use these two asteroseismic observables to identify for the first time an evolutionary sequence of 1 M-circle dot field stars, without the need for further information from stellar models. Comparison of our determinations with the few available spectroscopic results shows an excellent level of agreement. We discuss the potential of the method for differential analysis throughout the main-sequence evolution and the possibility of detecting twins of very well-known stars.
C1 [Aguirre, V. Silva; Weiss, A.; Casagrande, L.; Schoenrich, R.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
   [Chaplin, W. J.; Verner, G. A.; Miglio, A.; Broomhall, A. M.; Elsworth, Y.; Hekker, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
   [Ballot, J.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
   [Ballot, J.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, Toulouse, France.
   [Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
   [Bedding, T. R.; Huber, D.; Stello, D.; White, T. R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
   [Serenelli, A. M.] Fac Ciencies, Inst Ciencias Espacio CSIC IEEC, Bellaterra 08193, Spain.
   [Verner, G. A.] Queen Mary Univ London, Astron Unit, London E1 4NS, England.
   [Monteiro, M. J. P. F. G.; Campante, T. L.; Sousa, S. G.] Univ Porto, Ctr Astrophys, P-4150762 Oporto, Portugal.
   [Monteiro, M. J. P. F. G.; Campante, T. L.; Sousa, S. G.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
   [Appourchaux, T.; Gaulme, P.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
   [Bonanno, A.; Corsaro, E.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
   [Bruntt, H.; Campante, T. L.; Handberg, R.; Karoff, C.; Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
   [Garcia, R. A.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFI SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.
   [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
   [Mathur, S.; Metcalfe, T. S.; Thompson, M. J.] NCAR, High Altitude Observ, Boulder, CO 80307 USA.
   [Mosser, B.] Univ Paris 07, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92195 Meudon, France.
   [Salabert, D.] Univ Nice, CNRS, Observ Cote dAzur, F-06304 Nice 4, France.
   [White, T. R.] Australian Astron Observ, Epping, NSW 1710, Australia.
   [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA.
   [Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
   [Molenda-Zakowicz, J.] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland.
   [Caldwell, D. A.; Christiansen, J. L.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Wohler, B.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Aguirre, VS (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany.
RI Ballot, Jerome/G-1019-2010; Weiss, Achim/C-4870-2013; Sousa,
   Sergio/I-7466-2013; Monteiro, Mario J.P.F.G./B-4715-2008; Caldwell,
   Douglas/L-7911-2014; 
OI Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776;
   Serenelli, Aldo/0000-0001-6359-2769; Handberg,
   Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Weiss,
   Achim/0000-0002-3843-1653; Sousa, Sergio/0000-0001-9047-2965; Monteiro,
   Mario J.P.F.G./0000-0003-0513-8116; Karoff,
   Christoffer/0000-0003-2009-7965; Caldwell, Douglas/0000-0003-1963-9616;
   Bonanno, Alfio/0000-0003-3175-9776; Bedding,
   Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416
FU NASA's Science Mission Directorate; International Space Science
   Institute (ISSI)
FX Funding for this Discovery mission is provided by NASA's Science Mission
   Directorate. The authors thank the entire Kepler team, without whom
   these results would not be possible. We also thank all funding councils
   and agencies that have supported the activities of KASC Working Group 1.
   We are also grateful for support from the International Space Science
   Institute (ISSI).
NR 50
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2011
VL 740
IS 1
AR L2
DI 10.1088/2041-8205/740/1/L2
PG 7
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SC Astronomy & Astrophysics
GA 824OH
UT WOS:000295210900002
ER

PT J
AU Ferkinhoff, C
   Brisbin, D
   Nikola, T
   Parshley, SC
   Stacey, GJ
   Phillips, TG
   Falgarone, E
   Benford, DJ
   Staguhn, JG
   Tucker, CE
AF Ferkinhoff, Carl
   Brisbin, Drew
   Nikola, Thomas
   Parshley, Stephen C.
   Stacey, Gordon J.
   Phillips, Thomas G.
   Falgarone, Edith
   Benford, Dominic J.
   Staguhn, Johannes G.
   Tucker, Carol E.
TI FIRST DETECTIONS OF THE [N II] 122 mu m LINE AT HIGH REDSHIFT:
   DEMONSTRATING THE UTILITY OF THE LINE FOR STUDYING GALAXIES IN THE EARLY
   UNIVERSE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: high-redshift; galaxies: individual
   (SMMJ02399-136, H1413+117); galaxies: starburst; submillimeter: galaxies
ID FAR-INFRARED SPECTROSCOPY; QUASI-STELLAR OBJECTS; INTERSTELLAR-MEDIUM;
   CLOVERLEAF QUASAR; STAR-FORMATION; PHYSICAL CONDITIONS; MOLECULAR GAS;
   SUBMILLIMETER GALAXIES; O-III; STARBURST
AB We report the first detections of the [N II] 122 mu m line from a high-redshift galaxy. The line was strongly (>6 sigma) detected from SMMJ02399-0136, and H1413 + 117 (the Cloverleaf QSO) using the Redshift (z) and Early Universe Spectrometer on the Caltech Submillimeter Observatory. The lines from both sources are quite bright with line to far-infrared (FIR) continuum luminosity ratios that are similar to 7.0 x 10(-4) (Cloverleaf) and 2.1 x 10(-3) (SMMJ02399). With ratios 2-10 times larger than the average value for nearby galaxies, neither source exhibits the line-to-continuum deficits seen in nearby sources. The line strengths also indicate large ionized gas fractions, similar to 8%-17% of the molecular gas mass. The [O III]/[N II] line ratio is very sensitive to the effective temperature of ionizing stars and the ionization parameter for emission arising in the narrow-line region (NLR) of an active galactic nucleus (AGN). Using our previous detection of the [O III] 88 mu m line, the [O III]/[N II] line ratio for SMMJ02399-0136 indicates that the dominant source of the line emission is either stellar H II regions ionized by O9.5 stars, or the NLR of the AGN with ionization parameter log(U) = -3.3 to -4.0. A composite system, where 30%-50% of the FIR lines arise in the NLR also matches the data. The Cloverleaf is best modeled by a superposition of similar to 200 M82-like starbursts accounting for all of the FIR emission and 43% of the [N II] line. The remainder may come from the NLR. This work demonstrates the utility of the [N II] and [O III] lines in constraining properties of the ionized medium.
C1 [Ferkinhoff, Carl; Brisbin, Drew; Nikola, Thomas; Parshley, Stephen C.; Stacey, Gordon J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Phillips, Thomas G.] CALTECH, Pasadena, CA 91125 USA.
   [Falgarone, Edith] Observ Paris, CNRS, LERMA, Paris, France.
   [Falgarone, Edith] ENS, Paris, France.
   [Benford, Dominic J.; Staguhn, Johannes G.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab Code 665, Greenbelt, MD 20771 USA.
   [Staguhn, Johannes G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
   [Tucker, Carol E.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
RP Ferkinhoff, C (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM cferkinh@astro.cornell.edu
RI Benford, Dominic/D-4760-2012
OI Benford, Dominic/0000-0002-9884-4206
FU NSF [AST-00736289, AST-0722220]; NASA [NNX10AM09H]
FX This work was supported by NSF grants AST-00736289 and AST-0722220, and
   NASA grant NNX10AM09H. We thank the CSO staff for their support of ZEUS
   operations and the anonymous reviewer for their helpful comments.
NR 49
TC 25
Z9 25
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2011
VL 740
IS 1
AR L29
DI 10.1088/2041-8205/740/1/L29
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 824OH
UT WOS:000295210900029
ER

EF