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37 results on '"Gehrels, N."'

1. Fermi-LAT Observations of the Gamma-Ray Burst GRB 130427A

Author

Ackermann, M., Ajello, M., Asano, K., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Bechtol, K., Bellazzini, R., Bissaldi, E., Bonamente, E., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Burgess, J. Michael, Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Cecchi, C., Chaplin, V., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Chiaro, G., Ciprini, S., Claus, R., Cleveland, W., Cohen-Tanugi, J., Collazzi, A., Cominsky, L. R., Connaughton, V., Conrad, J., Cutini, S., D'Ammando, F., de Angelis, A., DeKlotz, M., de Palma, F., Dermer, C. D., Desiante, R., Diekmann, A., Di Venere, L., Drell, P. S., Drlica-Wagner, A., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Finke, J., Fitzpatrick, G., Focke, W. B., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gehrels, N., Germani, S., Gibby, M., Giglietto, N., Giles, M., Giordano, F., Giroletti, M., Godfrey, G., Granot, J., Grenier, I. A., Grove, J. E., Gruber, D., Guiriec, S., Hadasch, D., Hanabata, Y., Harding, A. K., Hayashida, M., Hays, E., Horan, D., Hughes, R. E., Inoue, Y., Jogler, T., Jóhannesson, G., Johnson, W. N., Kawano, T., Knödlseder, J., Kocevski, D., Kuss, M., Lande, J., Larsson, S., Latronico, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Mayer, M., Mazziotta, M. N., McEnery, J. E., Michelson, P. F., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Nemmen, R., Nuss, E., Ohno, M., Ohsugi, T., Okumura, A., Omodei, N., Orienti, M., Paneque, D., Pelassa, V., Perkins, J. S., Pesoe-Rollins, M., Petrosian, V., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L, Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ritz, S., Roth, M., Ryde, F., Sartori, A., Parkinson, P. M. Saz, Scargle, J. D., Schulz, A., Sgrò, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Tajima, H., Takahashi, H., Thayer, J. G., Thayer, J. A., Thompson, D. J., Tibaldo, L., Tinivella, M., Torres, D. F., Tosti, G., Troja, E., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Winer, B. L., Wood, K. S., Yamazaki, R., Younes, G., Yu, H.-F., Zhu, S. J., Bhat, P. N., Briggs, M. S., Byrne, D., Foley, S., Goldstein, A., Jenke, P., Kippen, R. M., Kouveliotou, C., McBreen, S., Meegan, C., Paciesas, W. S., Preece, R., Rau, A., Tierney, D., van der Horst, A. J., von Kienlin, A., Wilson-Hodge, C., Xiong, S., Cusumano, G., La Parola, V., and Cummings, J. R.

Published
2014
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2. GRB 130427A: A Nearby Ordinary Monster

Author

Maselli, A., Melandri, A., Nava, L., Mundell, C. G., Kawai, N., Campana, S., Covino, S., Cummings, J. R., Cusumano, G., Evans, P. A., Ghirlanda, G., Ghisellini, G., Guidorzi, C., Kobayashi, S., Kuin, P., La Parola, V., Mangano, V., Oates, S., Sakamoto, T., Serino, M., Virgili, F., Zhang, B.-B., Barthelmy, S., Beardmore, A., Bernardini, M. G., Bersier, D., Burrows, D., Calderone, G., Capalbi, M., Chiang, J., D'Avanzo, P., D'Elia, V., De Pasquale, M., Fugazza, D., Gehrels, N., Gomboc, A., Harrison, R., Hanayama, H., Japelj, J., Kennea, J., Kopac, D., Kouveliotou, C., Kuroda, D., Levan, A., Malesani, D., Marshall, F., Nousek, J., O'Brien, P., Osborne, J. P., Pagani, C., Page, K. L., Page, M., Perri, M., Pritchard, T., Romano, P., Saito, Y., Sbarufatti, B., Salvaterra, R., Steele, I., Tanvir, N., Vianello, G., Weigand, B., Wiersema, K., Yatsu, Y., Yoshii, T., and Tagliaferri, G.

Published
2014
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4. A Population of Gamma-Ray Millisecond Pulsars Seen with the Fermi Large Area Telescope

Author

Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Baughman, B. M., Bechtol, K., Bellazzini, R., Berenji, B., Bignami, G. F., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Carlson, P., Casandjian, J. M., Cecchi, C., Çelik, Ö., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cognard, I., Cohen-Tanugi, J., Cominsky, L. R., Conrad, J., Corbet, R., Cutini, S., Dermer, C. D., Desvignes, G., de Angelis, A., de Luca, A., de Palma, F., Digel, S. W., Dormody, M., Silva, E. do Couto e, Drell, P. S., Dubois, R., Dumora, D., Edmonds, Y., Farnier, C., Favuzzi, C., Fegan, S. J., Focke, W. B., Frailis, M., Freire, P. C. C., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giebels, B., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Hanabata, Y., Harding, A. K., Hayashida, M., Hays, E., Hobbs, G., Hughes, R. E., Jóhannesson, G., Johnson, A. S., Johnson, R. P., Johnson, T. J., Johnson, W. N., Johnston, S., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Knödlseder, J., Kocian, M. L., Kramer, M., Kuss, M., Lande, J., Latronico, L., Lemoine-Goumard, M., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Manchester, R. N., Marelli, M., Mazziotta, M. N., McConville, W., McEnery, J. E., McLaughlin, M. A., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce-Rollins, M., Piron, F., Porter, T. A., Rainò, S., Rando, R., Ransom, S. M., Ray, P. S., Razzano, M., Rea, N., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Roth, M., Ryde, F., Sadrozinski, H. F. W., Sanchez, D., Sander, A., Parkinson, P. M. Saz, Scargle, J. D., Schalk, T. L., Sgrò, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Stappers, B. W., Starck, J. L., Striani, E., Strickman, M. S., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. B., Thayer, J. G., Theureau, G., Thompson, D. J., Thorsett, S. E., Tibaldo, L., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Usher, T. L., Van Etten, A., Vasileiou, V., Venter, C., Vilchez, N., Vitale, V., Waite, A. P., Wallace, E., Wang, P., Watters, K., Webb, N., Weltevrede, P., Winer, B. L., Wood, K. S., Ylinen, T., and Ziegler, M.

Published
2009
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5. Detection of 16 Gamma-Ray Pulsars through Blind Frequency Searches Using the Fermi LAT

Author

Abdo, A. A., Ackermann, M., Ajello, M., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Baughman, B. M., Bechtol, K., Bellazzini, R., Berenji, B., Bignami, G. F., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Çelik, Ö., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Cutini, S., Dermer, C. D., de Angelis, A., de Luca, A., de Palma, F., Digel, S. W., Dormody, M., Silva, E. do Couto e, Drell, P. S., Dubois, R., Dumora, D., Farnier, C., Favuzzi, C., Fegan, S. J., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giebels, B., Giglietto, N., Giommi, P., Giordano, F., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M.-H., Grove, J. E., Guillemot, L., Guiriec, S., Gwon, C., Hanabata, Y., Harding, A. K., Hayashida, M., Hays, E., Hughes, R. E., Jóhannesson, G., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Knödlseder, J., Kocian, M. L., Kuss, M., Lande, J., Latronico, L., Lemoine-Goumard, M., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Marelli, M., Mazziotta, M. N., McConville, W., McEnery, J. E., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Parent, D., Pelassa, V., Pepe, M., Pesce-Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Primack, J. R., Rainò, S., Rando, R., Ray, P. S., Razzano, M., Rea, N., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Ryde, F., Sadrozinski, H. F.-W., Sanchez, D., Sander, A., Parkinson, P. M. Saz, Scargle, J. D., Sgrò, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Starck, J.-L., Strickman, M. S., Suson, D. J., Tajima, H., Takahashi, H., Takahashi, T., Tanaka, T., Thayer, J. G., Thompson, D. J., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Usher, T. L., Van Etten, A., Vasileiou, V., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Watters, K., Winer, B. L., Wolff, M. T., Wood, K. S., Ylinen, T., and Ziegler, M.

Published
2009
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6. The Fermi Large Area Telescope On Orbit: Event Classification, Instrument Response Functions, and Calibration

Author

Ackermann, M., Ajello, M., Albert, A., Allafort, A., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bloom, E. D., Bogart, J. R., Bonamente, E., Borgland, A. W., Bottacini, E., Bouvier, A., Brandt, T. J., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cavazzuti, E., Cecchi, C., Celik, O., Charles, E., Chaves, R. C. G., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Corbet, R., Cutini, S., D'Ammando, F., Davis, D. S., de, Angelis A., DeKlotz, M., de, Palma F., Dermer, C. D., Digel, S. W., do, Couto e Silva E., Drell, P. S., Drlica-Wagner, A., Dubois, R., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Fortin, P., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Giebels, B., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Hays, E., Horan, D., Hou, X., Hughes, R. E., Jackson, M. S., Jogler, T., Johannesson, G., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kerr, M., Knodlseder, J., Kuss, M., Lande, J., Larsson, S., Latronico, L., Lavalley, C., Lemoine-Goumard, M., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., McConville, W., McEnery, J. E., Mehault, J., Michelson, P. F., Mitthumsiri, W., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann-Godo, M., Nemmen, R., Norris, J. P., Nuss, E., Fukazawa, Yasushi, Hayashida, Masaaki, Kamae, Tsuneyoshi, Katagiri, Hideaki, Kataoka, Jun, Mizuno, Tsunefumi, Nishino, Sho, Ohno, Masanori, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), GLAST, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Ackermann, M., Ajello, M., Albert, A., Allafort, A., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., BARBIELLINI AMIDEI, Guido, Bastieri, D., Bechtol, K., Bellazzini, R., Bissaldi, Elisabetta, Blandford, R. D., Bloom, E. D., Bogart, J. R., Bonamente, E., Borgland, A. W., Bottacini, E., Bouvier, A., Brandt, T. J., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cavazzuti, E., Cecchi, C., Celik, ., Charles, E., R. C. G., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Corbet, R., Cutini, S., D'Ammando, F., Davis, D. S., Angelis, A., Deklotz, M., Palma, F., Dermer, C. D., Digel, S. W., E. d. C., Drell, P. S., Drlica Wagner, A., Dubois, R., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Fortin, P., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Giebels, B., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Hayashida, M., Hays, E., Horan, D., Hou, X., Hughes, R. E., Jackson, M. S., Jogler, T., Johannesson, G., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Kn\odlseder, J., Kuss, M., Lande, J., Larsson, S., Latronico, L., Lavalley, C., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mcconville, W., Mcenery, J. E., Mehault, J., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann Godo, M., Nemmen, R., Nishino, S., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Okumura, A., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Perkins, J. S., Pesce Rollins, M., Pierbattista, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rain\`o, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reposeur, T., Reyes, L. C., Ritz, S., Rochester, L. S., Romoli, C., Roth, M., Sadrozinski, H. F., Sanchez, D. A., Saz, P. M., Sbarra, C., Scargle, J. D., Sgr\`o, C., Siegal Gaskins, J., Siskind, E. J., Spandre, G., Spinelli, P., Stephens, T. E., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Thompson, D. J., Tibaldo, L., Tinivella, M., Tosti, G., Troja, E., Usher, T. L., Vandenbroucke, J., Klaveren, B., Vasileiou, V., Vianello, G., Vitale, V., Waite, A. P., Wallace, E., Winer, B. L., Wood, D. L., Wood, K. S., Wood, M., Yang, Z., Zimmer, S., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Ackermann M, Ajello M, Albert A, Allafort A, Atwood WB, Axelsson M, Baldini L, Ballet J, Barbiellini G, Bastieri D, Bechtol K, Bellazzini R, Bissaldi E, Blandford RD, Bloom ED, Bogart JR, Bonamente E, Borgland AW, Bottacini E, Bouvier A, Brandt TJ, Bregeon J, Brigida M, Bruel P, Buehler R, Burnett TH, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Casandjian JM, Cavazzuti E, Cecchi C, Celik O, Charles E, Chaves RCG, Chekhtman A, Cheung CC, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Conrad J, Corbet R, Cutini S, DAmmando F, Davis DS, de Angelis A, DeKlotz M, de Palma F, Dermer CD, Digel SW, Silva EDE, Drell PS, Drlica-Wagner A, Dubois R, Favuzzi C, Fegan SJ, Ferrara EC, Focke WB, Fortin P, Fukazawa Y, Funk S, Fusco P, Gargano F, Gasparrini D, Gehrels N, Giebels B, Giglietto N, Giordano F, Giroletti M, Glanzman T, Godfrey G, Grenier IA, Grove JE, Guiriec S, Hadasch D, Hayashida M, Hays E, Horan D, Hou X, Hughes RE, Jackson MS, Jogler T, Johannesson G, Johnson RP, Johnson TJ, Johnson WN, Kamae T, Katagiri H, Kataoka J, Kerr M, Knodlseder J, Kuss M, Lande J, Larsson S, Latronico L, Lavalley C, Lemoine-Goumard M, Longo F, Loparco F, Lott B, Lovellette MN, Lubrano P, Mazziotta MN, McConville W, McEnery JE, Mehault J, Michelson PF, Mitthumsiri W, Mizuno T, Moiseev AA, Monte C, Monzani ME, Morselli A, Moskalenko IV, Murgia S, Naumann-Godo M, Nemmen R, Nishino S, Norris JP, Nuss E, Ohno M, Ohsugi T, Okumura A, Omodei N, Orienti M, Orlando E, Ormes JF, Paneque D, Panetta JH, Perkins JS, Pesce-Rollins M, Pierbattista M, Piron F, Pivato G, Porter TA, Racusin JL, Raino S, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Reposeur T, Reyes LC, Ritz S, Rochester LS, Romoli C, Roth M, Sadrozinski HFW, Sanchez DA, Parkinson PMS, Sbarra C, Scargle JD, Sgro C, Siegal-Gaskins J, Siskind EJ, Spandre G, Spinelli P, Stephens TE, Suson DJ, Tajima H, Takahashi H, Tanaka T, Thayer JG, Thayer JB, Thompson DJ, Tibaldo L, Tinivella M, Tosti G, Troja E, Usher TL, Vandenbroucke J, Van Klaveren B, Vasileiou V, Vianello G, Vitale V, Waite AP, Wallace E, Winer BL, Wood DL, Wood KS, Wood M, Yang Z, and Zimmer S

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, observational [methods], instrumentation: detector, Instrumentation: detectors, instrumentation: miscellaneous, methods: data analysis, methods: observational, telescopes, 01 natural sciences, law.invention, Telescope, Spitzer Space Telescope, law, 0103 physical sciences, Calibration, 010303 astronomy & astrophysics, Remote sensing, Physics, 010308 nuclear & particles physics, detector [instrumentation], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], instrumentation: miscellaneou, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Gamma-ray astronomy, Space and Planetary Science, data analysi [methods], Orbit (dynamics), Data analysis, ddc:520, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, methods: data analysi, miscellaneou [instrumentation], Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

著者人数: 186名, Accepted: 2012-08-16, 資料番号: SA1004203000

Published
2012

7. The Fermi Large Area Telescope on Orbit: Event Classification, Instrument Response Functions

Author

Ackermann, M., Ajello, M., Albert, A., Allafort, A., Atwood, W. B., Axelsson, M., Baldini, Luca, Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bloom, E. D., Bogart, J. R., Bonamente, E., Borgland, A. W., Bottacini, E., Bouvier, A., Brandt, T. J., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cavazzuti, E., Cecchi, C., Çelik, Ö., Charles, E., Chaves, R. C. G., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Corbet, R., Cutini, S., D’Ammando, F., Davis, D. S., de Angelis, A., Deklotz, M., de Palma, F., Dermer, C. D., Digel, S. W., Silva, E. do Couto e., Drell, P. S., Drlica Wagner, A., Dubois, R., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Fortin, P., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Giebels, B., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Hayashida, M., Hays, E., Horan, D., Hou, X., Hughes, R. E., Jackson, M. S., Jogler, T., Jóhannesson, G., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Knödlseder, J., Kuss, M., Lande, J., Larsson, S., Latronico, L., Lavalley, C., Lemoine Goumard, M., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mcconville, W., Mcenery, J. E., Mehault, J., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann Godo, M., Nemmen, R., Nishino, S., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Okumura, A., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Perkins, J. S., Pesce Rollins, M., Pierbattista, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzano, Massimiliano, Razzaque, S., Reimer, A., Reimer, O., Reposeur, T., Reyes, L. C., Ritz, S., Rochester, L. S., Romoli, C., Roth, M., Sadrozinski, H. F. W., Sanchez, D. A., Saz Parkinson, P. M., Sbarra, C., Scargle, J. D., Sgrò, C., Siegal Gaskins, J., Siskind, E. J., Spandre, G., Spinelli, P., Stephens, T. E., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Thompson, D. J., Tibaldo, L., Tinivella, Marco, Tosti, G., Troja, E., Usher, T. L., Vandenbroucke, J., Van Klaveren, B., Vasileiou, V., Vianello, G., Vitale, V., Waite, A. P., Wallace, E., Winer, B. L., Wood, D. L., Wood, K. S., Wood, M., Yang, Z., and Zimmer, S.

Subjects
instrumentation: miscellaneous, instrumentation: detectors, telescopes, methods: observational, methods: data analysis
Published
2012

8. A real-time fast radio burst: polarization detection and multiwavelength follow-up.

Author

Petroff, E., Bailes, M., Barr, E. D., Barsdell, B. R., Bhat, N. D. R., Bian, F., Burke-Spolaor, S., Caleb, M., Champion, D., Chandra, P., Da Costa, G., Delvaux, C., Flynn, C., Gehrels, N., Greiner, J., Jameson, A., Johnston, S., Kasliwal, M. M., Keane, E. F., and Keller, S.

Subjects
SOLAR radio bursts, POLARIZATION (Nuclear physics), WAVELENGTHS, INTERSTELLAR medium, TELESCOPES
Abstract

Fast radio bursts (FRBs) are one of the most tantalizing mysteries of the radio sky; their progenitors and origins remain unknown and until now no rapid multiwavelength follow-up of an FRB has been possible. New instrumentation has decreased the time between observation and discovery from years to seconds, and enables polarimetry to be performed on FRBs for the first time. We have discovered an FRB (FRB 140514) in real-time on 2014 May 14 at 17:14:11.06 UTC at the Parkes radio telescope and triggered follow-up at other wavelengths within hours of the event. FRB 140514 was found with a dispersion measure (DM) of 562.7(6) cm-3 pc, giving an upper limit on source redshift of z ≲ 0.5. FRB 140514 was found to be 21 ± 7 per cent (3s) circularly polarized on the leading edge with a 1σ upper limit on linear polarization <10 per cent. We conclude that this polarization is intrinsic to the FRB. If there was any intrinsic linear polarization, as might be expected from coherent emission, then it may have been depolarized by Faraday rotation caused by passing through strong magnetic fields and/or high-density environments. FRB 140514 was discovered during a campaign to re-observe known FRB fields, and lies close to a previous discovery, FRB 110220; based on the difference in DMs of these bursts and time-on-sky arguments, we attribute the proximity to sampling bias and conclude that they are distinct objects. Follow-up conducted by 12 telescopes observing from X-ray to radio wavelengths was unable to identify a variable multiwavelength counterpart, allowing us to rule out models in which FRBs originate from nearby (z < 0.3) supernovae and long duration gamma-ray bursts. [ABSTRACT FROM AUTHOR]

Published
2015
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9. Blazar candidates beyond redshift 4 observed by Swift.

Author

Sbarrato, T., Ghisellini, G., Tagliaferri, G., Foschini, L., Nardini, M., Tavecchio, F., and Gehrels, N.

Subjects
BLACK holes, BL Lacertae objects, REDSHIFT, QUASARS, TELESCOPES, X-rays
Abstract

We have selected SDSS J222032.50+002537.5 and SDSS J142048.01+120545.9 as best blazar candidates out of a complete sample of extremely radio-loud quasars at z > 4, with highly massive black holes. We observed them and a third serendipitous candidate with similar features (PMN J2134-0419) in the X-rays with the Swift/XRT telescope, to confirm their blazar nature. We observed strong and hard X-ray fluxes (i.e. αX∼<0.6, where F(ν)∝ν-αX in the 0.3-10 keV observed energy range, ∼1-40 keV rest frame) in all three cases. This allowed us to classify our candidates as real blazars, being characterized by large Lorentz factors (∼13) and very small viewing angles (∼3°). All three sources have black hole masses exceeding 109 M⊙ and their classification provides intriguing constraints on supermassive black hole formation and evolution models. We confirm our earlier suggestion that there are different formation epochs of extremely massive black holes hosted in jetted (z ∼ 4) and non-jetted systems (z ∼ 2.5). [ABSTRACT FROM AUTHOR]

Published
2015
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10. Recent Progress on GRBs with Swift.

Author

Gehrels, N. and Cannizzo, J. K.

Subjects
*GAMMA ray bursts, *GAMMA ray astronomy, *ASTRONOMICAL observatories, *AFTERGLOW (Physics), *TELESCOPES, *SUPERNOVAE, *METAPHYSICAL cosmology
Abstract

We are in an exciting period of discovery for gamma-ray bursts. The Swift observatory is detecting 100 bursts per year, providing arcsecond localizations and sensitive observations of the prompt and afterglow emission. In addition, rapid-response telescopes on the ground have new capabilities to study optical emission during the prompt phase and spectral signatures of the host galaxies. The combined data set is enabling great advances in our understanding of GRBs including afterglow physics, short burst origin, and supernova physics. [ABSTRACT FROM AUTHOR]

Published
2010
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11. Prompt optical observations of GRB 080330 and GRB 080413A.

Author

Yuan, F., Rykoff, E. S., Schaefer, B. E., Rujopakarn, W., Güver, T., Aharonian, F., Akerlof, C. W., Ashley, M. C. B., Barthelmy, S. D., Gehrels, N., Gögăüş, E., Horns, D., Kizilogğlu, Ü., Krimm, H. A., Mckay, T. A., Özel, M., Phillips, A., Quimby, R. M., Rowell, G., and Swan, H. F.

Subjects
GAMMA ray bursts, TELESCOPES, X-rays, AFTERGLOW (Physics), ASTROPHYSICS
Abstract

We report on the results of rapid responses to GRB 080330 and GRB 080413A by the ROTSE-IIIb and ROTSE-IIIc telecopes. In both cases, optical follow-up started during the prompt emission phase and recorded optical flares peaking at similar times as the last hard X-ray pulses detected by the Swift BAT. For both events, the XRT observations started at the end of the prompt BAT detection and displayed an evolution in time opposite to the optical lightcurve. These very early observations provide us an opportunity to probe the onset of afterglow for these two events. [ABSTRACT FROM AUTHOR]

Published
2008
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12. Screening High-z GRBs with BAT Prompt Emission Properties.

Author

Ukwatta, T. N., Sakamoto, T., Stamatikos, M., Gehrels, N., and Dhuga, K. S.

Subjects
GAMMA ray bursts, TELESCOPES, ARTIFICIAL satellites, REDSHIFT, SPECTRUM analysis
Abstract

Detecting high-z GRBs is important for constraining the GRB formation rate, and tracing the history of re-ionization and metallicity of the universe. Based on the current sample of GRBs detected by Swift with known redshifts, we investigated the relationship between red-shift, and spectral and temporal characteristics, using the BAT event-by-event data. We found red-shift trends for the peak-flux-normalized temporal width T90, the light curve variance, the peak flux, and the photon index in simple power-law fit to the BAT event data. We have constructed criteria for screening GRBs with high red-shifts. This will enable us to provide a much faster alert to the GRB community of possible high-z bursts. [ABSTRACT FROM AUTHOR]

Published
2008
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13. GRBs with no afterglow even in the Swift Era?

Author

Vetere, L., Burrows, D. N., Gehrels, N., Meszaros, P., Morris, D. C., and Racusin, J. L.

Subjects
GAMMA ray bursts, AFTERGLOW (Physics), ARTIFICIAL satellites, X-rays, TELESCOPES
Abstract

Three years after its launch Swift has successfully localized and observed a few hundred GRBs. Its well-known speed in slewing to the source has led to great discoveries such as the flaring activities in early X-ray afterglows and the detection of Short GRB afterglows. In a few cases, mainly Short GRBs or late observations, XRT did not detect any emission. However, for six Long GRBs XRT could not measure any X-afterglow either, even as early as 100 s after the BAT trigger. In this paper we present a study of these unusual events. We analyse their peculiar behaviour in the Gamma and X-ray bands and discuss their singular origin. [ABSTRACT FROM AUTHOR]

Published
2008
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14. Extreme Properties of GRB 061007: a highly energetic or a highly collimated burst?

Author

Schady, P., De Pasquale, M., Page, M. J., Vetere, L., Wang, X. Y., Cummings, J., Zhang, B., Zane, S., Breeveld, A., Burrows, D. N., Gehrels, N., Gronwall, C., Hunsberger, S., Markwardt, C., Mason, K. O., Mészáros, P., Norris, J. P., Oates, S. R., Pagani, C., and Poole, T. S.

Subjects
GAMMA ray astronomy, AFTERGLOW (Physics), TELESCOPES, ARTIFICIAL satellites, SPACE astronomy
Abstract

GRB 061007 had the brightest optical afterglow observed by UVOT so far and a highly unusual afterglow light curve. It had an usually smooth and steep panchromatic temporal decay, which, from the start of the Swift observations, decayed as a power with a slope of α = 1.65±0.02 in the X-ray and UV/optical bands. If we interpret the data in terms of a spherical blastwave, the energy budget that is implied is enormous, challenging the possible models for the progenitors. The alternative explanation is that with GRB 061007 we are witnessing the most collimated outflow ever observed. If this is correct, if implies the occurrence of a jet break within 80 s of the prompt emission. This event has therefore remarkable consequences for the GRB communicate, since it may imply that jet breaks can occur much earlier in the afterglow light curves than hitherto expected. [ABSTRACT FROM AUTHOR]

Published
2008
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15. Improving Swift-XRT positions of GRBs.

Author

Evans, P. A., Beardmore, A. P., Goad, M. R., Osborne, J. P., Burrows, D. N., and Gehrels, N.

Subjects
X-ray telescopes, GAMMA ray bursts, DIGITAL cameras, METAPHYSICAL cosmology, TELESCOPES
Abstract

Since GRBs fade rapidly, it is important to publish accurate, precise positions at early times. For Swift-detected bursts, the best promptly available position is most commonly the X-ray Telescope (XRT) position. We present two processes, developed by the Swift team at Leicester, which are now routinely used to improve the precision and accuracy of the XRT positions reported by the Swift team. Both methods, which are fully automated, make use of a PSF-fitting approach which accounts for the bad columns on the CCD. The first method yields positions with 90% error radii <4.4″90% of the time, within 10–20 minutes of the trigger. The second method astrometrically corrects the position using UVOT field stars and the known mapping between the XRT and UVOT detectors, yielding enhanced positions with 90% error radii of <2.8″90% of the time, usually 2 hours after the trigger. [ABSTRACT FROM AUTHOR]

Published
2008
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16. The Swift Gamma-Ray Burst Mission.

Author

Gehrels, N.

Subjects
*ASTRONOMICAL observatories, *OBSERVATORIES, *GAMMA ray telescopes, *ASTRONOMICAL instruments, *GAMMA rays, *TELESCOPES, *ASTROPHYSICS, *ASTRONOMY, *PHYSICS
Abstract

Swift is a first-of-its-kind multiwavelength transient observatory for GRB astronomy. It has the optimum capabilities for the next breakthroughs in determining the origin of GRBs and their afterglows, as well as using bursts to probe the early Universe. Swift will also perform the first sensitive hard X-ray survey of the sky. The mission is being developed by an international collaboration and consists of three instruments, the Burst Alert Telescope (BAT), the X-ray Telescope (XRT), and the Ultraviolet and Optical Telescope (UVOT). The BAT, a wide-field gamma-ray detector, will detect > 100 GRBs per year with a sensitivity >2 times that of BATSE. The sensitive narrow-field XRT and UVOT will be autonomously slewed to the burst location in 20 to 75 seconds to determine 0.3–5.0 arcsec positions and perform optical, UV, and X-ray spectrophotometry. Strong education/public outreach and follow-up programs will help to engage the public and astronomical community. The Swift launch is planned for mid 2004. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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17. Swift Burst Alert Telescope (BAT) Instrument Response.

Author

Parsons, A., Barthelmy, S., Cummings, J., Gehrels, N., Hullinger, D., Krimm, H., Markwardt, C., Tueller, J., Fenimore, E., Palmer, D., Sato, G., Takahashi, T., Nakazawa, K., Okada, Y., Takahashi, H., Suzuki, M., and Tashiro, M.

Subjects
TELESCOPES, ASTRONOMICAL instruments, OPTICAL instruments, GAMMA ray bursts, GAMMA ray astronomy, ASTRONOMY
Abstract

The Burst Alert Telescope (BAT), a large coded aperture instrument with a wide field-of-view (FOV), provides the gamma-ray burst triggers and locations for the Swift Gamma-Ray Burst Explorer. In addition to providing this imaging information, BAT will perform a 15 keV – 150 keV all-sky hard x-ray survey based on the serendipitous pointings resulting from the study of gamma-ray bursts, and will also monitor the sky for transient hard x-ray sources. For BAT to provide spectral and photometric information for the gamma-ray bursts, the transient sources and the all-sky survey, the BAT instrument response must be determined to an increasingly greater accuracy. This paper describes the spectral models and the ground calibration experiments used to determine the BAT response to an accuracy suitable for gamma-ray burst studies. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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18. Setting the Triggering Thresholds on Swift.

Author

McLean, Kassandra M., Fenimore, E. E., Palmer, David, Barthelmy, S., Gehrels, N., Krimm, H., Markwardt, C., and Parsons, A.

Subjects
TELESCOPES, ASTRONOMICAL instruments, OPTICAL instruments, GAMMA ray bursts, GAMMA ray astronomy, ASTRONOMY
Abstract

The Burst Alert Telescope (BAT) on Swift has two main types of “rate” triggers: short and long. Short trigger time scales range from 4ms to 64ms, while long triggers are 64ms to ≈ 16 seconds. While both short and long trigger have criteria with one background sample (traditional “one-sided” triggers), the long triggers can also have criteria with two background samples (“bracketed” triggers) which remove trends in the background. Both long and short triggers can select energy ranges of 15–25, 15–50, 25–100 and 50–350 KeV. There are more than 180 short triggering criteria and approximately 500 long triggering criteria used to detect gamma ray bursts. To fully utilize these criteria, the thresholds must be set correctly. The optimum thresholds are determined by a tradeoff between avoiding false triggers and capturing as many bursts as possible. We use realistic simulated orbital variations, which are the prime cause of false triggers. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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19. The BAT-Swift Science Software.

Author

Palmer, D. M., Fenimore, E., Galassi, M., McLean, K., Tavenner, T., Barthelmy, S., Blau, M., Cummings, J., Gehrels, N., Hullinger, D., Krimm, H., Markwardt, C., Mason, R., Ong, J., Polk, J., Parsons, A., Shackelford, L., Tueller, J., Walling, S., and Okada, Y.

Subjects
TELESCOPES, ASTRONOMICAL instruments, OPTICAL instruments, GAMMA ray bursts, GAMMA ray astronomy, ASTRONOMY, COMPUTER software
Abstract

The BAT instrument tells Swift where to point to make immediate follow-up observations of GRBs. The science software on board must efficiently process γ-ray events coming in at up to 34 kHz, identify rate increases that could be due to GRBs while disregarding those from known sources, and produce images to accurately and rapidly locate new Gamma-ray sources. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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20. Observing GRBs with EXIST.

Author

Hartmann, D. H., Grindlay, J., Hong, J., Loeb, A., Blandford, R., Craig, W., Fishman, J., Kouveliotou, C., Gehrels, N., Band, D., Harrison, F., and Woosley, S. E.

Subjects
TELESCOPES, ASTRONOMICAL instruments, OPTICAL instruments, COSMOLOGICAL distances, STAR formation, GAMMA ray bursts, GAMMA ray astronomy
Abstract

We describe the Energetic X-ray Imaging Survey Telescope EXIST, designed to carry out a sensitive all-sky survey in the 10 keV – 600 keV band. The primary goal of EXIST is to find black holes in the local and distant universe. EXIST also traces cosmic star formation via gamma-ray bursts and gamma-ray lines from radioactive elements ejected by supernovae and novae. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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21. Super-LOTIS/LOTIS/LITE: Prompt GRB followup experiments.

Author

Park, H. S., Ables, E., Barthelmy, S., Bradshaw, M., Cline, T., Gehrels, N., Hartmann, D., Hurley, K., Nemiroff, R., Pereira, W., Perez-Ramirez, D., Williams, G. G., and Ziock, K.

Subjects
TELESCOPES, GAMMA ray bursts, IMAGING systems in astronomy, PHYSICAL optics
Abstract

LOTIS (Livermore Optical Transient Imaging System) and Super-LOTIS are automatic telescope systems that measure very prompt optical emission occurring within seconds of the gamma-ray energy release during a Gamma Ray Burst (GRB). Unlike hour-todays delayed afterglow measurements, very early measurements will contain information about the GRB progenitor. To accomplish this, we developed and have been operating automated telescopes that rapidly image GRB coordinate error boxes in response to triggers distributed by the GRB Coordinate Distribution Network (GCN). LOTIS, located in California, consists of 4 cameras each with a different astronomical filter (B, V, R, open) that can respond to GRB triggers within 5 s. Super-LOTIS can point to any part of the sky within 30 s upon receipt of a GCN trigger and its sensitivity is as deep as V=17~19 depending on the integration times. Since the shutdown of the CGRO, there has been no real-time GRB triggers that enable the LOTIS systems to measure real-time GRB counterpart fluxes as of May 2001. This paper describes performance of these systems. We also present our plan to replace the current optical CCD camera on the Super-LOTIS to a near infrared camera to be able to probe dusty GRB environment. [ABSTRACT FROM AUTHOR]

Published
2001

22. IAC-11.A7.2.1: Gamma-ray astronomy technology needs

Author

Gehrels, N. and Cannizzo, J.K.

Subjects
*GAMMA ray astronomy, *ASTRONOMICAL observations, *GAMMA ray bursts, *NUCLEOSYNTHESIS, *ACTIVE galactic nuclei, *ASTROPHYSICS
Abstract

Abstract: In recent decades observations have become a valuable tool for studying the universe. Progress made in diverse areas such as gamma-ray bursts (GRBs), nucleosynthesis, and active galactic nuclei (AGNs) has complemented and enriched our astrophysical understanding in many ways. We present an overview of current and future planned space missions and discuss technology needs for the next generation of space instruments. [Copyright &y& Elsevier]

Published
2012
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23. PheniX: a new vision for the hard X-ray sky.

Author

Roques, Jean-Pierre, Jourdain, Elisabeth, Bassani, Loredana, Bazzano, Angela, Belmont, Renaud, Bird, A., Caroli, E., Chauvin, M., Clark, D., Gehrels, N., Goerlach, U., Harrisson, F., Laurent, P., Malzac, J., Medina, P., Merloni, A., Paltani, S., Stephen, J., Ubertini, P., and Wilms, J.

Subjects
X-ray astronomy, TELESCOPES, MATHEMATICAL optimization, EMISSION spectroscopy, COMPACT objects (Astronomy), COMPTON effect, EQUATIONS of state
Abstract

We are proposing a mission devoted to high energy X-ray astronomy that is based on a focusing telescope operating in the 1-200 keV energy range but optimized for the hard X-ray range. The main scientific topics concern: Physics of compact objects: The proximity of compact objects provides a unique laboratory to study matter and radiation in extreme conditions of temperature and density in strong gravitational environment. The emission of high energy photons from these objects is far from being understood. The unprecedented sensitivity in the high energy domain will allow a precise determination of the non-thermal processes at work in the vicinity of compact objects. The full 1-200 keV energy coverage will be ideal to disentangle the emission processes produced in the spacetime regions most affected by strong-gravity, as well as the physical links: disk-thermal emission-iron line-comptonisation-reflection-non-thermal emission-jets. Neutron stars-magnetic field-cyclotron lines: Time resolved spectroscopy (and polarimetry) at ultra-high sensitivity of AXP, milliseconds pulsars and magnetars will give new tools to study the role of the synchrotron processes at work in these objects. Cyclotron lines-direct measurement of magnetic filed-equation of state constraints-short bursts-giant flares could all be studied with great details. AGN: The large sensitivity improvement will provide detailed spectral properties of the high energy emission of AGN's. This will give a fresh look to the connection between accretion and jet emission and will provide a new understanding of the physical processes at work. Detection of high-redshift active nuclei in this energy range will allow to introduce an evolutionary aspect to high-energy studies of AGN, probing directly the origin of the Cosmic X-ray Background also in the non-thermal range (> 20 keV). Element formation-Supernovae: The energy resolution achievable for this mission (<0.5 keV) and a large high energy effective area are ideally suited for the 44Ti line study (68 and 78 keV). This radioactive nuclei emission will give an estimate of their quantities and speed in their environment. In addition the study of the spatial structure and spectral emission of SNR will advance our knowledge of the dynamics of supernovae explosions, of particles acceleration mechanisms and how the elements are released in the interstellar medium. Instrumental design: The progress of X-ray focusing optics techniques allows a major step in the instrumental design: the collecting area becomes independent of the detection area. This drastically reduces the instrumental background and will open a new era. The optics will be based on depth-graded multi-layer mirrors in a Wolter I configuration. To obtain a significant effective area in the hundred of keV range a focal length in the 40-50 meters range (attainable with a deployable mast) is needed. In addition such a mission could benefit from recent progress made on mirror coating. We propose to cover the 1-200 keV energy range with a single detector, a double-sided Germanium strip detector operating at 80 K. The main features will be: (a) good energy resolution (.150 keV at 5 keV and <.5 keV at 100 keV), (b) 3 dimensional event localization with a low number of electronic chains, (c) background rejection by the 3D localization, (d) polarisation capabilities in the Compton regime. [ABSTRACT FROM AUTHOR]

Published
2012
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24. THE 60 MONTH ALL-SKY BURST ALERT TELESCOPE SURVEY OF ACTIVE GALACTIC NUCLEUS AND THE ANISOTROPY OF NEARBY AGNs.

Author

AJELLO, M., ALEXANDER, D. M., GREINER, J., MADEJSKI, G. M., GEHRELS, N., and BURLON, D.

Subjects
ACTIVE galactic nuclei, TELESCOPES, SKY, LUMINOSITY, DENSITY
Abstract

Surveys above 10 keV represent one of the best resources to provide an unbiased census of the population of active galactic nuclei (AGNs). We present the results of 60 months of observation of the hard X-ray sky with Swift/Burst Alert Telescope (BAT). In this time frame, BAT-detected (in the 15-55 keV band) 720 sources in an all-sky survey of which 428 are associated with AGNs, most of which are nearby. Our sample has negligible incompleteness and statistics a factor of ~2 larger over similarly complete sets of AGNs. Our sample contains (at least) 15 bona fide Compton-thick AGNs and 3 likely candidates. Compton-thick AGNs represent ~5% of AGN samples detected above 15 keV. We use the BAT data set to refine the determination of the log N-log S of AGNs which is extremely important, now that NuSTAR prepares for launch, toward assessing the AGN contribution to the cosmic X-ray background. We show that the log N-log S of AGNs selected above 10 keV is now established to ~10% precision. We derive the luminosity function of Compton-thick AGNs and measure a space density of 7.9-2.9+4.1 x 10-5 Mpc-3 for objects with a de-absorbed luminosity larger than 2 x 1042 erg s-1. As the BAT AGNs are all mostly local, they allow us to investigate the spatial distribution of AGNs in the nearby universe regardless of absorption. We find concentrations of AGNs that coincide spatially with the largest congregations of matter in the local (≤85 Mpc) universe. There is some evidence that the fraction of Seyfert 2 objects is larger than average in the direction of these dense regions. [ABSTRACT FROM AUTHOR]

Published
2012
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25. FERMI AND SWIFT GAMMA-RAY BURST AFTERGLOW POPULATION STUDIES.

Author

RACUSIN, J. L., OATES, S. R., SCHADY, P., BURROWS, D. N., DE PASQUALE, M., DONATO, D., GEHRELS, N., KOCH, S., MCENERY, J., PIRAN, T., ROMING, P., SAKAMOTO, T., SWENSON, C., TROJA, E., VASILEIOUF, V., WANDERMAN, VIRGIL D., and ZHANG, B.

Subjects
GAMMA rays, TELESCOPES, ASTRONOMY, GAMMA ray bursts, X-ray bursts, GAMMA ray astronomy
Abstract

The new and extreme population of gamma-ray bursts (GRBs) detected by the Fermi Large Area Telescope (LAT) shows several new features in high-energy gamma rays that are providing interesting and unexpected clues into GRB prompt and afterglow emission mechanisms. Over the last six years, it has been Swift that has provided the robust data set of UV/optical and X-ray afterglow observations that opened many windows into components of GRB emission structure. The relationship between the LAT-detected GRBs and the well-studied, fainter, and less energetic GRBs detected by the Swift Burst Alert Telescope is only beginning to be explored by multi-wavelength studies. We explore the large sample of GRBs detected by BAT only, BAT and the Fermi Gamma-ray Burst Monitor (GBM), and GBM and LAT, focusing on these samples separately in order to search for statistically significant differences between the populations, using only those GRBs with measured redshifts in order to physically characterize these objects. We disentangle which differences are instrumental selection effects versus intrinsic properties in order to better understand the nature of the special characteristics of the LAT bursts. [ABSTRACT FROM AUTHOR]

Published
2011
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26. GAMMA-RAY BURSTS — OBSERVATIONS.

Author

GEHRELS, N. and CANNIZZO, J. K.

Subjects
*GAMMA ray bursts, *GAMMA ray astronomy, *ELECTRIC discharges, *TELESCOPES, *ASTRONOMY
Abstract

We are in an exciting period of discovery for gamma-ray bursts. The Swift observatory is detecting 100 bursts per year, providing arcsecond localizations and sensitive observations of the prompt and afterglow emission. The Fermi observatory is observing 250 bursts per year with its medium-energy GRB instrument and about 10 bursts per year with its high-energy LAT instrument. In addition, rapid-response telescopes on the ground are providing new capabilities to study optical emission during the prompt phase and spectral signatures of the host galaxies. The combined data set is enabling great advances in our understanding of GRBs including afterglow physics, short burst origin, and high-energy emission. [ABSTRACT FROM AUTHOR]

Published
2010
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27. The 2008 May burst activation of SGR 1627–41.

Author

Esposito, P., Israel, G. L., Zane, S., Senziani, F., Starling, R. L. C., Rea, N., Palmer, D. M., Gehrels, N., Tiengo, A., De Luca, A., Götz, D., Mereghetti, S., Romano, P., Sakamoto, T., Barthelmy, S. D., Stella, L., Turolla, R., Feroci, M., and Mangano, V.

Subjects
GAMMA rays, TELESCOPES, ASTRONOMICAL instruments, EMISSIONS (Air pollution), SPECTRUM analysis
Abstract

In 2008 May, the soft gamma-ray repeater (SGR) SGR 1627−41 resumed its bursting activity after nearly a decade of quiescence. After detection of a bright burst, Swift pointed its X-ray telescope in the direction of the source in less than five hours and followed it for over five weeks. In this Letter, we present an analysis of the data from these Swift observations and an XMM–Newton one performed when SGR 1627−41 was still in a quiescent state. The analysis of the bursts detected with Swift/Burst Alert Telescope shows that their temporal and spectral properties are similar to those found in previous observations of SGR 1627−41 and other SGRs. The maximum peak luminosity of the bursts was . Our data show that the outburst was accompanied by a fast flux enhancement and by a hardening of the spectrum with respect to the persistent emission. [ABSTRACT FROM AUTHOR]

Published
2008
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28. The nature of the outflow in gamma-ray bursts.

Author

Kumar, P., McMahon, E., Panaitescu, A., Willingale, R., O'Brien, P., Burrows, D., Cummings, J., Gehrels, N., Holland, S., Pandey, S. B., Vanden Berk, D., and Zane, S.

Subjects
NATURAL satellites, TELESCOPES, SOLAR system, ASTROPHYSICS, ASTRONOMY
Abstract

The Swift satellite has enabled us to follow the evolution of gamma-ray burst (GRB) fireballs from the prompt γ-ray emission to the afterglow phase. The early-time X-ray and optical data for GRBs obtained by telescopes aboard the Swift satellite show that the source for prompt γ-ray emission, the emission that heralds these bursts, is short lived, and is distinct from the source for the long-lived afterglow emission that follows the initial burst. Using these data we determine the distance of the γ-ray source from the centre of the explosion. We find this distance to be 1015–1016 cm for most bursts, and show that this is within a factor of about 10 of the radius of the shock heated circumstellar medium (CSM) producing the X-ray photons. Furthermore, using the early γ-ray, X-ray and optical data we show that the prompt gamma-ray emission cannot be produced in internal shocks nor can it be produced in the external shock; in a more general sense γ-ray generation mechanisms based on shock physics have problems explaining the GRB data for ten Swift bursts analyzed in this work. A magnetic field dominated outflow model for GRBs has a number of attractive features, although evidence in its favour is inconclusive. Finally, the X-ray and optical data allow us to provide an upper limit on the density of the CSM of about 10 protons cm−3 at a distance of from the centre of explosion. [ABSTRACT FROM AUTHOR]

Published
2007
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29. The Swift γ-ray burst mission

Author

Gehrels, N.

Subjects
*GAMMA ray bursts, *GAMMA ray astronomy, *TELESCOPES, *AFTERGLOW (Physics), *GAMMA ray detectors
Abstract

Swift is a first-of-its-kind multiwavelength transient observatory for GRB astronomy. It has the optimum capabilities for the next breakthroughs in determining the origin of GRBs and their afterglows, as well as using bursts to probe the early Universe. Swift will also perform the first sensitive hard X-ray survey of the sky. The mission is being developed by an international collaboration and consists of three instruments, the Burst Alert Telescope (BAT), the X-Ray Telescope (XRT), and the Ultraviolet and Optical Telescope (UVOT). The BAT, a wide-field γ-ray detector, will detect >100 GRBs per year with a sensitivity five times that of BATSE. The sensitive narrow-field XRT and UVOT will be autonomously slewed to the burst location in 20–75 s to determine 0.3–5.0′′ positions and perform optical, UV, and X-ray spectrophotometry. Strong education/public outreach and follow-up programs will help to engage the public and astronomical community. The Swift launch is planned for 2004. [Copyright &y& Elsevier]

Published
2004
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30. Investigating the Possibility of Screening High-z GRBs based on BAT Prompt Emission Properties.

Author

Ukwatta, T. N., Sakamoto, T., Dhuga, K. S., Parke, W. C., Barthelmy, S. D., Gehrels, N., Stamatikos, M., and Tueller, J.

Subjects
GAMMA ray bursts, ARTIFICIAL satellites, REDSHIFT, TELESCOPES, METAPHYSICAL cosmology
Abstract

Being able to quickly select among gamma-ray bursts (GRBs) seen by the Swift satellite those which are high-z candidates would give ground-based observers a better chance to determine a redshift for such distant GRBs. Information about these high-z GRBs is important in helping to resolve questions about the early universe such as the formation rate of high-z GRBs, the re-ionization period of the universe, the metallicity of the early universe, and the Hubble expansion. Initially using a sample of 51 GRBs with previously measured redshifts, we have developed high-z screening criteria employing the GRB spectral as well as temporal characteristics of the prompt emission from the Burst Alert Telescope (BAT) on Swift. Now that the sample has increased to 81 GRBs, we have revisited the screening criteria and our methodology. Our updated high-z screening criteria are presented in this paper. [ABSTRACT FROM AUTHOR]

Published
2009
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31. Super-LOTIS and LOTIS for HETE2 GRB Triggers.

Author

Park, H. S., Williams, G. G., Ables, E., Barthelmy, S. D., Cline, T., Gehrels, N., Hartmann, D., Hurley, K., Lindsay, K., Nemiroff, R., Pereira, W., and Perez-Ramirez, D.

Subjects
TELESCOPES, GAMMA ray bursts, GAMMA ray astronomy
Abstract

LOTIS (Livermore Optical Transient Imaging System) and Super-LOTIS are automatic telescope systems that search for prompt optical emission from gamma-ray bursts (GRBs). Both systems are capable of responding to the Gamma-ray burst Coordinate Network (GCN) triggers within seconds. These systems have been monitoring the GCN real-time data for automatic HETE2 GRB triggers since HETE2's launch. In this paper, we present the systems' capability and current status. We also present the result of the GRB010921 afterglow detection that was localized by HETE2 and the IPN. [ABSTRACT FROM AUTHOR]

Published
2003

32. CHANDRA X-RAY OBSERVATIONS OF THE TWO BRIGHTEST UNIDENTIFIED HIGH GALACTIC LATITUDE FERMI-LAT γ-RAY SOURCES.

Author

Cheung, C. C., Donato, D., Gehrels, N., Sokolovsky, K. V., and Giroletti, M.

Subjects
GALACTIC cosmic rays, GALACTIC X-ray sources, WAVELENGTHS, TELESCOPES, MICROWAVE reflectometry
Abstract

We present Chandra ACIS-I X-ray observations of 0FGL J1311.9–3419 and 0FGL J1653.4–0200, the two brightest high Galactic latitude (|b| >10°) γ-ray sources from the three-month Fermi Large Area Telescope (LAT) bright source list that are still unidentified. Both were also detected previously by EGRET, and despite dedicated multi-wavelength follow-up, they are still not associated with established classes of γ-ray emitters like pulsars or radio-loud active galactic nuclei. X-ray sources found in the ACIS-I fields of view are cataloged, and their basic properties are determined. These are discussed as candidate counterparts to 0FGL J1311.9–3419 and 0FGL J1653.4–0200, with particular emphasis on the brightest of the 9 and 13 Chandra sources detected within the respective Fermi-LAT 95% confidence regions. Further follow-up studies, including optical photometric and spectroscopic observations, are necessary to identify these X-ray candidate counterparts in order to ultimately reveal the nature of these enigmatic γ-ray objects. [ABSTRACT FROM AUTHOR]

Published
2012
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35. Goddard Robotic Telescope – Optical follow-up of GRBs and coordinated observations of AGNs

Author

Sakamoto, T., Wallace, C.A., Donato, D., Gehrels, N., Okajima, T., and Ukwatta, T.N.

Subjects
*GAMMA ray bursts, *TELESCOPES, *ACTIVE galactic nuclei, *ASTRONOMICAL observations, *ASTRONOMICAL observatories, *ACQUISITION of data, *ROBOTICS
Abstract

Abstract: Since it is not possible to predict when a Gamma-Ray Burst (GRB) will occur or when Active Galactic Nucleus (AGN) flaring activity starts, follow-up/monitoring ground telescopes must be located as uniformly as possible all over the world in order to collect data simultaneously with Fermi and Swift detections. However, there is a distinct gap in follow-up coverage of telescopes in the eastern U.S. region based on the operations of Swift. Motivated by this fact, we have constructed a 14″ fully automated optical robotic telescope, Goddard Robotic Telescope (GRT), at the Goddard Geophysical and Astronomical Observatory. The aims of our robotic telescope are (1) to follow-up Swift/Fermi GRBs and (2) to perform the coordinated optical observations of Fermi Large Area Telescope (LAT) AGN. Our telescope system consists of off-the-shelf hardware. With the focal reducer, we are able to match the field of view of Swift narrow instruments (20′×20′). We started scientific observations in mid-November 2008 and GRT has been fully remotely operated since August 2009. The 3σ upper limit in a 30s exposure in the R filter is ∼15.4mag; however, we can reach to ∼18mag in a 600s exposures. Due to the weather condition at the telescope site, our observing efficiency is 30–40% on average. [Copyright &y& Elsevier]

Published
2011
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37. THE LARGE AREA TELESCOPE ON THEFERMI GAMMA-RAY SPACE TELESCOPEMISSION

Author

Atwood1, W. B., Abdo2, A. A., Ackermann3, M., Althouse3, W., Anderson1, B., Axelsson4, M., Baldini5, L., Ballet6, J., Band7, D. L., 8, Barbiellini9, G., Bartelt3, J., Bastieri11, D., Baughman13, B. M., Bechtol3, K., Bédérède14, D., Bellardi5, F., Bellazzini5, R., Berenji3, B., Bignami15, G. F., Bisello11, D., Bissaldi16, E., Blandford3, R. D., Bloom3, E. D., Bogart3, J. R., Bonamente, Emanuele, Bonnell8, J., Borgland3, A. W., Bouvier3, A., Bregeon5, J., Brez5, A., Brigida19, M., Bruel21, P., Burnett22, T. H., Busetto11, G., Caliandro19, G. A., Cameron3, R. A., Caraveo23, P. A., Carius24, S., Carlson25, P., Casandjian6, J. M., Cavazzuti26, E., Ceccanti5, M., Cecchi, Claudia, Charles3, E., Chekhtman2, A., Cheung8, C. C., Chiang3, J., Chipaux28, R., Cillis8, A. N., Ciprini17, S., Claus3, R., Cohen Tanugi29, J., Condamoor3, S., Conrad25, J., Corbet8, R., Corucci5, L., Costamante3, L., Cutini26, S., Davis8, D. S., Decotigny21, D., Deklotz32, M., Dermer2, C. D., de Angelis33, A., Digel3, S. W., Silva3, E. do Couto e., Drell3, P. S., Dubois3, R., Dumora34, D., Edmonds3, Y., Fabiani5, D., Farnier29, C., Favuzzi19, C., Flath3, D. L., Fleury21, P., Focke3, W. B., Funk3, S., Fusco19, P., Gargano20, F., Gasparrini26, D., Gehrels8, N., Gentit37, F. X., Germani17, S., Giebels21, B., Giglietto19, N., Giommi26, P., Giordano19, F., Glanzman3, T., Godfrey3, G., Grenier6, I. A., Grondin34, M. H., Grove2, J. E., Guillemot34, L., Guiriec29, S., Haller3, G., Harding8, A. K., Hart3, P. A., Hays8, E., Healey3, S. E., Hirayama8, M., Hjalmarsdotter4, L., Horn32, R., Hughes13, R. E., Jóhannesson3, G., Johansson24, G., Johnson3, A. S., Johnson1, R. P., Johnson8, T. J., Johnson2, W. N., Kamae3, T., Katagiri38, H., Kataoka39, J., Kavelaars3, A., Kawai40, N., Kelly3, H., Kerr22, M., Klamra25, W., Knödlseder41, J., Kocian3, M. L., Komin6, N., Kuehn13, F., Kuss5, M., Landriu6, D., Latronico5, L., Lee42, B., Lee3, S. H., Lemoine Goumard34, M., Lionetto43, A. M., Longo9, F., Loparco19, F., Lott34, B., Lovellette2, M. N., Lubrano17, P., Madejski3, G. M., Makeev27, A., 2, Marangelli19, B., Massai5, M. M., Mazziotta20, M. N., Mcenery8, J. E., Menon5, N., Meurer30, C., Michelson3, P. F., Minuti5, M., Mirizzi19, N., Mitthumsiri3, W., Mizuno38, T., Moiseev7, A. A., Monte19, C., Monzani3, M. E., Moretti9, E., Morselli43, A., Moskalenko3, I. V., Murgia3, S., Nakamori39, T., Nishino38, S., Nolan3, P. L., Norris45, J. P., Nuss29, E., Ohno46, M., Ohsugi38, T., Omodei5, N., Orlando16, E., Ormes45, J. F., Paccagnella11, A., Paneque3, D., Panetta3, J. H., Parent34, D., Pearce25, M., Pepe17, M., Perazzo3, A., Pesce Rollins5, M., Picozza43, P., Pieri11, L., Pinchera5, M., Piron29, F., Porter1, T. A., Poupard6, L., Rainò19, S., Rando11, R., Rapposelli5, E., Razzano5, M., Reimer3, A., Reimer3, O., Reposeur34, T., Reyes48, L. C., Ritz8, S., Rochester3, L. S., Rodriguez49, A. Y., Romani3, R. W., Roth22, M., Russell3, J. J., Ryde25, F., Sabatini43, S., Sadrozinski1, H. F. W., Sanchez21, D., Sander13, A., Sapozhnikov3, L., Saz Parkinson1, P. M., Scargle50, J. D., Schalk1, T. L., Scolieri51, G., Sgrò5, C., Share2, G. H., Shaw3, M., Shimokawabe39, T., Shrader7, C., Sierpowska Bartosik49, A., Siskind53, E. J., Smith34, D. A., Smith13, P. D., Spandre5, G., Spinelli19, P., Starck6, J. L., Stephens8, T. E., Strickman2, M. S., Strong16, A. W., Suson54, D. J., Tajima3, H., Takahashi38, H., Takahashi46, T., Tanaka3, T., Tenze5, A., Tether3, S., Thayer3, J. B., Thayer3, J. G., Thompson8, D. J., Tibaldo11, L., Tibolla55, O., Torres56, D. F., Tosti, Gino, Tramacere57, A., 3, Turri3, M., Usher3, T. L., Vilchez41, N., Vitale43, V., Wang3, P., Watters3, K., Winer13, B. L., Wood2, K. S., Ylinen24, T., Ziegler1, M., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Fermi-LAT, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Atwood, W. B., Abdo, A. A., Ackermann, M., Althouse, W., Anderson, B., Axelsson, M., Baldini, L., Ballet, J., Band, D. L., BARBIELLINI AMIDEI, Guido, Bartelt, J., Bastieri, D., Baughman, B. M., Bechtol, K., Bederede, D., Bellardi, F., Bellazzini, R., Berenji, B., Bignami, G. F., Bisello, D., Bissaldi, Elisabetta, Blandford, R. D., Bloom, E. D., Bogart, J. R., Bonamente, E., Bonnell, J., Borgland, A. W., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Busetto, G., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Carius, S., Carlson, P., Casandjian, J. M., Cavazzuti, E., Ceccanti, M., Cecchi, C., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Chipaux, R., Cillis, A. N., Ciprini, S., Claus, R., Cohen Tanugi, J., Condamoor, S., Conrad, J., Corbet, R., Corucci, L., Costamante, L., Cutini, S., Davis, D. S., Decotigny, D., Deklotz, M., Dermer, C. D., Angelis, A. D., Digel, S. W., Silva, E. D. C. E., Drell, P. S., Dubois, R., Dumora, D., Edmonds, Y., Fabiani, D., Farnier, C., Favuzzi, C., Flath, D. L., Fleury, P., Focke, W. B., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Gentit, F. X., Germani, S., Giebels, B., Giglietto, N., Giommi, P., Giordano, F., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Haller, G., Harding, A. K., Hart, P. A., Hays, E., Healey, S. E., Hirayama, M., Hjalmarsdotter, L., Horn, R., Hughes, R. E., Johannesson, G., Johansson, G., Johnson, A. S., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kavelaars, A., Kawai, N., Kelly, H., Kerr, M., Klamra, W., Knodlseder, J., Kocian, M. L., Komin, N., Kuehn, F., Kuss, M., Landriu, D., Latronico, L., Lee, B., Lee, S. H., Lemoine Goumard, M., Lionetto, A. M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Marangelli, B., Massai, M. M., Mazziotta, M. N., Mcenery, J. E., Menon, N., Meurer, C., Michelson, P. F., Minuti, M., Mirizzi, N., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Nishino, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paccagnella, A., Paneque, D., Panetta, J. H., Parent, D., Pearce, M., Pepe, M., Perazzo, A., Pesce Rollins, M., Picozza, P., Pieri, L., Pinchera, M., Piron, F., Porter, T. A., Poupard, L., Raino, S., Rando, R., Rapposelli, E., Razzano, M., Reimer, A., Reimer, O., Reposeur, T., Reyes, L. C., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Roth, M., Russell, J. J., Ryde, F., Sabatini, S., Sadrozinski, H. F. W., Sanchez, D., Sander, A., Sapozhnikov, L., Parkinson, P. M. S., Scargle, J. D., Schalk, T. L., Scolieri, G., Sgro, C., Share, G. H., Shaw, M., Shimokawabe, T., Shrader, C., Sierpowska Bartosik, A., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Starck, J. L., Stephens, T. E., Strickman, M. S., Strong, A. W., Suson, D. J., Tajima, H., Takahashi, H., Takahashi, T., Tanaka, T., Tenze, A., Tether, S., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Turri, M., Usher, T. L., Vilchez, N., Vitale, V., Wang, P., Watters, K., Winer, B. L., Wood, K. S., Ylinen, T., Ziegler, M., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Fermi satellite, Astrophysics, Gamma rays: observations, Tracking (particle physics), 01 natural sciences, High Energy Gamma-ray Astronomy, law.invention, Telescope, Spitzer Space Telescope, Cosmic rays, Galaxies: active, Galaxy: general, Sun: X-rays, gamma rays, Telescopes, law, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, Calorimeter (particle physics), 010308 nuclear & particles physics, GRB 080916C, GRB 130427A, Detectors, Astronomy and Astrophysics, gamma rays, Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Sun: X-rays, Fermi Gamma-ray Space Telescope
Abstract

著者人数：240名, Accepted: 2009-03-19, 資料番号: SA1000971000

Published
2009

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