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51. The origin of the early-time optical emission of Swift GRB 080310★.

Author

Littlejohns, O. M., Willingale, R., O'Brien, P. T., Beardmore, A. P., Covino, S., Perley, D. A., Tanvir, N. R., Rol, E., Yuan, F., Akerlof, C., D'Avanzo, P., Bersier, D. F., Castro-Tirado, A. J., Christian, P., Cobb, B. E., Evans, P. A., Filippenko, A. V., Flewelling, H., Fugazza, D., and Hoversten, E. A.

Subjects
GAMMA ray bursts, FIELD emission, WAVELENGTHS, ASTRONOMICAL observations, REDSHIFT, EXTRAPOLATION, INFRARED astronomy
Abstract

ABSTRACT We present broad-band multiwavelength observations of GRB 080310 at redshift z= 2.43. This burst was bright and long-lived, and unusual in having extensive optical and near-infrared (IR) follow-up during the prompt phase. Using these data we attempt to simultaneously model the gamma-ray, X-ray, optical and IR emission using a series of prompt pulses and an afterglow component. Initial attempts to extrapolate the high-energy model directly to lower energies for each pulse reveal that a spectral break is required between the optical regime and 0.3 keV to avoid overpredicting the optical flux. We demonstrate that afterglow emission alone is insufficient to describe all morphology seen in the optical and IR data. Allowing the prompt component to dominate the early-time optical and IR and permitting each pulse to have an independent low-energy spectral indices we produce an alternative scenario which better describes the optical light curve. This, however, does not describe the spectral shape of GRB 080310 at early times. The fit statistics for the prompt- and afterglow-dominated models are nearly identical making it difficult to favour either. However one enduring result is that both models require a low-energy spectral index consistent with self-absorption for at least some of the pulses identified in the high-energy emission model. [ABSTRACT FROM AUTHOR]

Published
2012
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52. Two years of monitoring supergiant fast X-ray transients with Swift.

Author

Romano, P., La Parola, V., Vercellone, S., Cusumano, G., Sidoli, L., Krimm, H. A., Pagani, C., Esposito, P., Hoversten, E. A., Kennea, J. A., Page, K. L., Burrows, D. N., and Gehrels, N.

Subjects
SUPERGIANT stars, PHOTONS, GAS bursts, X-ray binaries, NEUTRONS, STELLAR luminosity function
Abstract

We present results based on 2 yr of intense Swift monitoring of three supergiant fast X-ray transients (SFXTs), IGR J 16479−4514, XTE J 1739−302 and IGR J 17544−2619, which we started in 2007 October. Our out-of-outburst intensity-based X-ray (0.3-10 keV) spectroscopy yields absorbed power laws characterized by hard photon indices ( Γ∼ 1 -2). The broad-band (0.3-150 keV) spectra of these sources, obtained while they were undergoing new outbursts observed during the second year of monitoring, can be fitted well with models typically used to describe the X-ray emission from accreting neutron stars in high-mass X-ray binaries. We obtain an assessment of how long each source spends in each state using a systematic monitoring with a sensitive instrument. By considering our monitoring as a casual sampling of the X-ray light curves, we can infer that the time these sources spend in bright outbursts is between 3 and 5 per cent of the total. The most probable X-ray flux for these sources is ∼ (1 -2) × 10−11 erg cm−2 s−1 (2-10 keV, unabsorbed), corresponding to luminosities of the order of a few 1033 to a few 1034 erg s−1 (two orders of magnitude lower than the bright outbursts). In particular, the duty-cycle of inactivity is ∼19, 39 and 55 per cent (∼5 per cent uncertainty) for IGR J 16479−4514, XTE J 1739−302 and IGR J 17544−2619, respectively. We present a complete list of BAT onboard detections, which further confirm the continued activity of these sources. This demonstrates that true quiescence is a rare state and that these transients accrete matter throughout their life at different rates. Variability in the X-ray flux is observed at all time-scales and intensity ranges we can probe. Superimposed on the day-to-day variability is intraday flaring, which involves flux variations up to one order of magnitude that can occur down to time-scales as short as ∼1 ks, and which can be naturally explained by the accretion of single clumps composing the donor wind with masses Mcl∼ (0.3 -2) × 1019 g. Thanks to the Swift observations, the general picture we obtain is that, despite individual differences, common X-ray characteristics of this class are now well defined, such as outburst lengths well in excess of hours, with a multiple peaked structure, and a high dynamic range (including bright outbursts), up to approximately four orders of magnitude. [ABSTRACT FROM AUTHOR]

Published
2011
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53. GRB 081203A: Swift UVOT captures the earliest ultraviolet spectrum of a gamma-ray burst.

Author

Kuin, N. P. M., Landsman, W., Page, M. J., Schady, P., Still, M., Breeveld, A. A., De Pasquale, M., Roming, P. W. A., Brown, P. J., Carter, M., James, C., Curran, P. A., Cucchiara, A., Gronwall, C., Holland, S. T., Hoversten, E. A., Hunsberger, S., Kennedy, T., Koch, S., and Lamoureux, H.

Subjects
ULTRAVIOLET radiation, GAMMA ray bursts, GALAXIES, REDSHIFT, ASTRONOMICAL instruments, ASTRONOMICAL research
Abstract

We present the earliest ultraviolet (UV) spectrum of a gamma-ray burst (GRB) as observed with the Swift Ultra-Violet/Optical Telescope (UVOT). The GRB 081203A spectrum was observed for 50 s with the UV-grism starting 251 s after the Swift-Burst-Alert-Telescope (BAT) trigger. During this time, the GRB was ≈13.4 mag ( u filter) and was still rising to its peak optical brightness. In the UV-grism spectrum, we find a damped Lyα line, Lyβ and the Lyman continuum break at a redshift . A model fit to the Lyman absorption implies a gas column density of log , which is typical of GRB host galaxies with damped Lyα absorbers. This observation of GRB 081203A demonstrates that for brighter GRBs with moderate redshift the UVOT is able to provide redshifts, and probe for damped Lyα absorbers within 4–6 min from the time of the Swift-BAT trigger. [ABSTRACT FROM AUTHOR]

Published
2009
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54. A statistical study of gamma-ray burst afterglows measured by the Swift Ultraviolet Optical Telescope.

Author

Oates, S. R., Page, M. J., Schady, P., de Pasquale, M., Koch, T. S., Breeveld, A. A., Brown, P. J., Chester, M. M., Holland, S. T., Hoversten, E. A., Kuin, N. P. M., Marshall, F. E., Roming, P. W. A., Still, M., Vanden Berk, D. E., Zane, S., and Nousek, J. A.

Subjects
GAMMA ray bursts, GAMMA ray astronomy, GAMMA rays, LIGHT curves, STELLAR luminosity function, X-ray telescopes
Abstract

We present the first statistical analysis of 27 Ultraviolet Optical Telescope (UVOT) optical/ultraviolet light curves of gamma-ray burst (GRB) afterglows. We have found, through analysis of the light curves in the observer's frame, that a significant fraction rise in the first 500 s after the GRB trigger, all light curves decay after 500 s, typically as a power law with a relatively narrow distribution of decay indices, and the brightest optical afterglows tend to decay the quickest. We find that the rise could be either produced physically by the start of the forward shock, when the jet begins to plough into the external medium, or geometrically where an off-axis observer sees a rising light curve as an increasing amount of emission enters the observers line of sight, which occurs as the jet slows. We find that at 99.8 per cent confidence, there is a correlation, in the observed frame, between the apparent magnitude of the light curves at 400 s and the rate of decay after 500 s. However, in the rest frame, a Spearman rank test shows only a weak correlation of low statistical significance between luminosity and decay rate. A correlation should be expected if the afterglows were produced by off-axis jets, suggesting that the jet is viewed from within the half-opening angle θ or within a core of a uniform energy density . We also produced logarithmic luminosity distributions for three rest-frame epochs. We find no evidence for bimodality in any of the distributions. Finally, we compare our sample of UVOT light curves with the X-ray Telescope (XRT) light-curve canonical model. The range in decay indices seen in UVOT light curves at any epoch is most similar to the range in decay of the shallow decay segment of the XRT canonical model. However, in the XRT canonical model, there is no indication of the rising behaviour observed in the UVOT light curves. [ABSTRACT FROM AUTHOR]

Published
2009
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57. Communications satellites: Looking to the 1980s: It will be a decade of new and exciting applications, lower costs, and more reliable service

Author

Van Trees, H. L., Hoversten, E. V., and McGarty, T. P.

Abstract

How will satellite communications evolve in the decade 1980–1990? In answer to that question, some prognostications appear reasonably certain of fulfillment: • The INTELSAT global communications system will continue to grow, providing existing services at lower cost and introducing new services. • Domestic and regional systems will continue to expand. • The Space Transportation System will have a major impact. • Technological advances will allow systems with complexity and capability probably an order of magnitude greater than present-day systems. • Applications will expand from classical point-to-point telephony and broadcast into many new areas.

Published
1977
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58. Swift Observation of GRB 110808A

Author

Stratta, G., Valerio D'Elia, Gendre, B., Pritchard, T. A., Sakamoto, T., Barthelmy, S. D., Burrows, D. N., Hoversten, E. A., and Gehrels, N.

62. Multiwavelength observations of mrk 501 in 2008

Author

Kranich, D., Paneque, D., Cesarini, A., Falcone, A., Giroletti, M., Hoversten, E., Hovatta, T., Yuri Kovalev, Lähteenmäki, A., Nieppola, E., Pagani, C., Pichel, A., Satalecka, K., Scargle, J., Steele, D., Tavecchio, F., Tescaro, D., Tornikoski, M., and Villata, M.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The well-studied VHE (E >100 GeV) blazar Mrk 501 was observed between March and May 2008 as part of an extensive multiwavelength observation campaign including radio, optical, X-ray and VHE gamma-ray instruments. Mrk 501 was in a low state of activity during the campaign, with a low VHE flux of about 20% the Crab Nebula flux. Nevertheless, significant flux variations could be observed in X-rays as well as $\gamma$-rays. Overall Mrk 501 showed increased variability when going from radio to gamma-ray energies. The broadband spectral energy distribution during the two different emission states of the campaign was well described by a homogeneous one-zone synchrotron self-Compton model. The high emission state was satisfactorily modeled by increasing the amount of high energy electrons with respect to the low emission state. This parameterization is consistent with the energy-dependent variability trend observed during the campaign., Comment: Contribution to the 31st ICRC, Lodz, Poland, July 2009

65. Swift and Fermi observations of the early afterglow of the short Gamma-Ray Burst 090510

Author

M. De Pasquale, P. Schady, N. P. M. Kuin, M. J. Page, P. A. Curran, S. Zane, S. R. Oates, S. T. Holland, A. A. Breeveld, E. A. Hoversten, G. Chincarini, D. Grupe, A. A. Abdo, M. Ackermann, M. Ajello, M. Axelsson, L. Baldini, J. Ballet, G. Barbiellini, M. G. Baring, D. Bastieri, K. Bechtol, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, E. D. Bloom, E. Bonamente, A. W. Borgland, A. Bouvier, J. Bregeon, A. Brez, M. S. Briggs, M. Brigida, P. Bruel, T. H. Burnett, S. Buson, G. A. Caliandro, R. A. Cameron, P. A. Caraveo, S. Carrigan, J. M. Casandjian, C. Cecchi, Ö. Çelik, A. Chekhtman, J. Chiang, S. Ciprini, R. Claus, J. Cohen-Tanugi, V. Connaughton, J. Conrad, C. D. Dermer, A. de Angelis, F. de Palma, B. L. Dingus, E. do Couto e Silva, P. S. Drell, R. Dubois, D. Dumora, C. Farnier, C. Favuzzi, S. J. Fegan, G. Fishman, W. B. Focke, M. Frailis, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, D. Gasparrini, N. Gehrels, S. Germani, N. Giglietto, F. Giordano, T. Glanzman, G. Godfrey, J. Granot, J. Greiner, I. A. Grenier, J. E. Grove, L. Guillemot, S. Guiriec, A. K. Harding, M. Hayashida, E. Hays, D. Horan, R. E. Hughes, M. S. Jackson, G. Jóhannesson, A. S. Johnson, W. N. Johnson, T. Kamae, H. Katagiri, J. Kataoka, N. Kawai, M. Kerr, R. M. Kippen, J. Knödlseder, D. Kocevski, M. Kuss, J. Lande, L. Latronico, M. Lemoine-Goumard, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, A. Makeev, M. N. Mazziotta, J. E. McEnery, S. McGlynn, C. Meegan, P. Mészáros, C. Meurer, P. F. Michelson, W. Mitthumsiri, T. Mizuno, C. Monte, M. E. Monzani, E. Moretti, A. Morselli, I. V. Moskalenko, S. Murgia, P. L. Nolan, J. P. Norris, E. Nuss, M. Ohno, T. Ohsugi, N. Omodei, E. Orlando, J. F. Ormes, W. S. Paciesas, D. Paneque, J. H. Panetta, D. Parent, V. Pelassa, M. Pepe, M. Pesce-Rollins, F. Piron, T. A. Porter, R. Preece, S. Rainò, R. Rando, M. Razzano, A. Reimer, O. Reimer, T. Reposeur, S. Ritz, L. S. Rochester, A. Y. Rodriguez, M. Roth, F. Ryde, H. F.-W. Sadrozinski, A. Sander, P. M. Saz Parkinson, J. D. Scargle, T. L. Schalk, C. Sgrò, E. J. Siskind, P. D. Smith, G. Spandre, P. Spinelli, M. Stamatikos, J.-L. Starck, F. W. Stecker, M. S. Strickman, D. J. Suson, H. Tajima, H. Takahashi, T. Tanaka, J. B. Thayer, J. G. Thayer, D. J. Thompson, L. Tibaldo, K. Toma, D. F. Torres, G. Tosti, A. Tramacere, Y. Uchiyama, T. Uehara, T. L. Usher, A. J. van der Horst, V. Vasileiou, N. Vilchez, V. Vitale, A. von Kienlin, A. P. Waite, P. Wang, B. L. Winer, K. S. Wood, X. F. Wu, R. Yamazaki, T. Ylinen, M. Ziegler, 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), 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 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 (UB)-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), 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), Fermi-LAT, 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), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), 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, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Pasquale, M. D., Schady, P., Kuin, N. P. M., Page, M. J., Curran, P. A., Zane, S., Oates, S. R., Holland, S. T., Breeveld, A. A., Hoversten, E. A., Chincarini, G., Grupe, D., Abdo, A. A., Ackermann, M., Ajello, M., Axelsson, M., Baldini, L., Ballet, J., BARBIELLINI AMIDEI, Guido, Baring, M. G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bissaldi, Elisabetta, Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bouvier, A., Bregeon, J., Brez, A., Briggs, M. S., Brigida, M., Bruel, P., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Carrigan, S., Casandjian, J. M., Cecchi, C., Celik, O., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Connaughton, V., Conrad, J., Dermer, C. D., Angelis, A. d., Palma, F. d., Dingus, B. L., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Farnier, C., Favuzzi, C., Fegan, S. J., Fishman, G., Focke, W. B., Frailis, M., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Granot, J., Greiner, J., Grenier, I. A., Grove, J. E., Guillemot, L., Guiriec, S., Harding, A. K., Hayashida, M., Hays, E., Horan, D., Hughes, R. E., Jackson, M. S., Johannesson, G., Johnson, A. S., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Kippen, R. M., Knodlseder, J., Kocevski, D., Kuss, M., Lande, J., Latronico, L., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Makeev, A., Mazziotta, M. N., Mcenery, J. E., Mcglynn, S., Meegan, C., Meszaros, P., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paciesas, W. S., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce Rollins, M., Piron, F., Porter, T. A., Preece, R., Raino, S., Rando, R., Razzano, M., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Roth, M., Ryde, F., Sadrozinski, H. F. W., Sander, A., Parkinson, P. M. S., Scargle, J. D., Schalk, T. L., Sgro, C., Siskind, E. J., Smith, P. D., Spandre, G., Spinelli, P., Stamatikos, M., Starck, J. L., Stecker, F. W., Strickman, M. S., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Toma, K., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Uehara, T., Usher, T. L., van der Horst, A. J., Vasileiou, V., Vilchez, N., Vitale, V., Kienlin, A. v., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., X. F., Wu, Yamazaki, R., Ylinen, T., and Ziegler, M.

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma-ray burst: individual (GRB090510), relativistic processes, shock waves, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Fermi satellite, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, High Energy Gamma-ray Astronomy, gamma-ray burst: individual (GRB090510), Spitzer Space Telescope, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, gamma-ray burst: individual: GRB090510, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], GRB 080916C, Astronomy and Astrophysics, Afterglow, Shock (mechanics), Space and Planetary Science, Gamma-ray Bursts, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract

We present the observations of GRB090510 performed by the Fermi Gamma-Ray Space Telescope and the Swift observatory. This is a bright, short burst that shows an extended emission detected in the GeV range. Furthermore, its optical emission initially rises, a feature so far observed only in long bursts, while the X-ray flux shows an initial shallow decrease, followed by a steeper decay. This exceptional behavior enables us to investigate the physical properties of the GRB outflow, poorly known in short bursts. We discuss internal shock and external shock models for the broadband energy emission of this object., Comment: Comments: Submitted to ApJ Letters. Contact Authors: Massimiliano De Pasquale (mdp@mssl.ucl.ac.uk), Mathew Page (mjp@mssl.ucl.ac.uk), Kenji Toma (toma@astro.psu.edu), Veronique Pelassa (pelassa@lpta.in2p3.fr). Minor change in the authorlist

Published
2009
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66. PKS 1502+106: a new and distant gamma-ray blazar in outburst discovered by the Fermi Large Area Telescope

Author

Abdo1, A. A., 2, Ackermann3, M., Ajello3, M., Atwood4, W. B., Axelsson5, M., 6, Baldini7, L., Ballet8, J., Barbiellini9, G., Bastieri11, D., Baughman13, B. M., Bechtol3, K., Bellazzini7, R., Berenji3, B., Bloom3, E. D., Bogaert14, G., Bonamente, Emanuele, Borgland3, A. W., Bregeon7, J., Brez7, A., Brigida17, M., Bruel14, P., Burnett19, T. H., Caliandro20, G. A., Cameron3, R. A., Caraveo21, P. A., Casandjian8, J. M., Cavazzuti22, E., Cecchi, Claudia, Çelik23, Ö., 25, 24, Chekhtman1, A., Cheung1, C. C., Chiang3, J., Ciprini16, S., Claus3, R., Cohen Tanugi27, J., Conrad6, J., 66, 28, Cutini22, S., Dermer1, C. D., de Angelis29, A., de Palma17, F., Digel3, S. W., Silva3, E. do Couto e., Drell3, P. S., Dubois3, R., Dumora30, D., Farnier27, C., Favuzzi17, C., Fegan14, S. J., Ferrara23, E. C., Focke3, W. B., Frailis29, M., Fuhrmann32, L., Fukazawa33, Y., Funk3, S., Fusco17, P., Gargano18, F., Gasparrini22, D., Gehrels23, N., 35, 34, Germani15, S., Giebels14, B., Giglietto17, N., Giordano17, F., Giroletti36, M., Glanzman3, T., Godfrey3, G., Grenier8, I. A., Grondin30, M. H., Grove1, J. E., Guillemot32, L., Guiriec37, S., Hanabata33, Y., Harding23, A. K., Hayashida3, M., Hays23, E., Hughes13, R. E., Jóhannesson3, G., Johnson3, A. S., Johnson4, R. P., Johnson1, W. N., Kadler24, M., 39, 38, Kamae3, T., Katagiri33, H., Kataoka41, J., Kerr19, M., Knödlseder42, J., Kocian3, M. L., Kuehn13, F., Kuss7, M., Lande3, J., Latronico7, L., Lemoine Goumard30, M., Longo9, F., Loparco17, F., Lott30, B., Lovellette1, M. N., Lubrano15, P., Madejski3, G. M., Makeev1, A., Marelli21, M., Massaro43, E., Max Moerbeck44, W., Mazziotta18, M. N., Mcconville23, W., Mcenery23, J. E., Meurer6, C., Michelson3, P. F., Mitthumsiri3, W., Mizuno33, T., Moiseev24, A. A., Monte17, C., Monzani3, M. E., Morselli45, A., Moskalenko3, I. V., Murgia3, S., Nolan3, P. L., Norris46, J. P., Nuss27, E., Ohsugi33, T., Omodei7, N., Orlando47, E., Ormes46, J. F., Ozaki48, M., Paneque3, D., Panetta3, J. H., Parent30, D., Pavlidou44, V., Pearson44, T. J., Pelassa27, V., Pepe15, M., Pesce Rollins7, M., Piron27, F., Porter4, T. A., Rainò17, S., Rando11, R., Razzano7, M., Razzaque1, S., Readhead44, A., Reimer3, A., Reimer3, O., Reposeur30, T., Richards44, J. L., Ritz4, S., Rochester3, L. S., Rodriguez20, A. Y., Romani3, R. W., Roth19, M., Ryde6, F., Sadrozinski4, H. F. W., Sanchez14, D., Sander13, A., Saz Parkinson4, P. M., Scargle51, J. D., Sgrò7, C., Shaw3, M. S., Siskind52, E. J., Smith30, D. A., Smith13, P. D., Spandre7, G., Spinelli17, P., Stevenson44, M., Strickman1, M. S., Suson53, D. J., Tajima3, H., Takahashi33, H., Tanaka3, T., Thayer3, J. B., Thayer3, J. G., Thompson23, D. J., Tibaldo8, L., 12, 11, Tibolla54, O., Torres20, D. F., Tosti, Gino, Tramacere3, A., Ubertini57, P., Uchiyama3, Y., Usher3, T. L., Vasileiou24, V., Vilchez42, N., Vitale45, V., Waite3, A. P., Wang3, P., Winer13, B. L., Wood1, K. S., Yasuda33, H., Ylinen6, T., 59, 50, Zensus32, J. A., Ziegler4, M., Angelakis32, E., Hovatta60, T., Hoversten34, E., Ikejiri33, Y., Kawabata61, K. S., Kovalev32, Y. Y., Kovalev62, Y. u. A., Krichbaum32, T. P., Lister63, M. L., Lähteenmäki60, A., Marchili32, N., Ogle44, P., Pagani34, C., Pushkarev32, A. B., 65, 64, Sakimoto33, K., Sasada33, M., Tornikoski60, M., Uemura61, M., Yamanaka33, M., Yamashita61, T., 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), 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 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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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, Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Baughman, B. M., Bechtol, K., Bellazzini, R., Berenji, B., Bloom, E. D., Bogaert, G., 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., Cavazzuti, E., Cecchi, C., Celik, O., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Cutini, S., Dermer, C. D., Angelis, A. d., Palma, F. d., Digel, S. W., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Farnier, C., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Frailis, M., Fuhrmann, L., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giebels, B., Giglietto, N., Giordano, F., Giroletti, M., 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., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, W. N., Kadler, M., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Knodlseder, J., Kocian, M. L., Kuehn, F., Kuss, M., Lande, J., Latronico, L., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Marelli, M., Massaro, E., Max Moerbeck, W., Mazziotta, M. N., Mcconville, W., Mcenery, J. E., 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., Ozaki, M., Paneque, D., Panetta, J. H., Parent, D., Pavlidou, V., Pearson, T. J., Pelassa, V., Pepe, M., Pesce Rollins, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Razzano, M., Razzaque, S., Readhead, A., Reimer, A., Reimer, O., Reposeur, T., Richards, J. L., 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. S., Scargle, J. D., Sgro, C., Shaw, M. S., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Stevenson, M., Strickman, M. S., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Ubertini, P., Uchiyama, Y., Usher, T. L., Vasileiou, V., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Yasuda, H., Ylinen, T., Zensus, J. A., Ziegler, M., Angelakis, E., Hovatta, T., Hoversten, E., Ikejiri, Y., Kawabata, K. S., Kovalev, Y. Y., Kovalev, Y. A., Krichbaum, T. P., Lister, M. L., Lahteenmaki, A., Marchili, N., Ogle, P., Pagani, C., Pushkarev, A. B., Sakimoto, K., Sasada, M., Tornikoski, M., Uemura, M., Yamanaka, M., Yamashita, T., 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 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 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), and 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)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], quasars: individual (PKS 1502+106), Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Gamma-ray Astronomy, Fermi satellite, Active Galactic Nuclei, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), galaxies: active, galaxies: jets, gamma rays: general, quasars: general, quasars: individual: PKS 1502+106, X-rays: galaxies, Galaxies: active, 01 natural sciences, General Relativity and Quantum Cosmology, Luminosity, law.invention, Telescope, Spitzer Space Telescope, law, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Astronomy and Astrophysics, Quasar, Space and Planetary Science, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数：207名, Accepted: 2009-12-21, 資料番号: SA1000987000

Published
2009
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