%0 Journal Article
%T The Spectral Energy Distribution of Fermi bright blazars
%+ Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))
%+ Laboratoire Leprince-Ringuet (LLR)
%+ Laboratoire de Physique Théorique et Astroparticules (LPTA)
%+ Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG)
%+ Centre d'étude spatiale des rayonnements (CESR)
%A Abdo, A.A.
%A Ackermann, Markus
%A Ajello, Marco
%A Axelsson, Magnus
%A Baldini, Luca
%A Ballet, Jean
%A Barbiellini, Guido
%A Bastieri, D.
%A Baughman, B.M.
%A Bechtol, K.
%A Bellazzini, R.
%A Berenji, B.
%A Blandford, R.D.
%A Bloom, E.D.
%A Bonamente, E.
%A Borgland, A.
%A Bregeon, J.
%A Brez, A.
%A Brigida, M.
%A Bruel, Pascal
%A Burnett, T. H.
%A Buson, S.
%A Caliandro, G. A.
%A Cameron, R. A.
%A Caraveo, P. A.
%A Casandjian, J. M.
%A Cavazzuti, E.
%A Cecchi, C.
%A Celik, O.
%A Charles, E.
%A Chaty, S.
%A Chekhtman, A.
%A Chiang, J.
%A Ciprini, S.
%A Claus, R.
%A Cohen-Tanugi, J.
%A Colafrancesco, S.
%A Cominsky, L. R.
%A Conrad, J.
%A Costamante, L.
%A Cutini, S.
%A Dermer, C. D.
%A de Angelis, A.
%A de Palma, F.
%A Digel, S. W.
%A Silva, E. Do Couto E
%A Drell, P. S.
%A Dubois, R.
%A Dumora, D.
%A Farnier, C.
%A Favuzzi, C.
%A Fegan, S. J.
%A Focke, W. B.
%A Fortin, P.
%A Frailis, M.
%A Fuhrmann, L.
%A Fukazawa, Y.
%A Funk, S.
%A Fusco, P.
%A Gargano, F.
%A Gasparrini, D.
%A Gehrels, N.
%A Germani, S.
%A Giebels, B.
%A Giglietto, N.
%A Giommi, P.
%A Giordano, F.
%A Glanzman, T.
%A Godfrey, G.
%A Grenier, I. A.
%A Grove, J. E.
%A Guillemot, L.
%A Guiriec, S.
%A Hadasch, D.
%A Hanabata, Y.
%A Harding, A. K.
%A Hayashida, M.
%A Hays, E.
%A Healey, S. E.
%A Horan, D.
%A Hughes, R. E.
%A Itoh, R.
%A Jackson, M. S.
%A Johannesson, G.
%A Johnson, A. S.
%A Johnson, W. N.
%A Kadler, M.
%A Kamae, T.
%A Katagiri, H.
%A Kataoka, J.
%A Kawai, N.
%A Kerr, M.
%A Knödlseder, Jürgen
%A Kocian, M. L.
%A Kuss, M.
%A Lande, J.
%A Latronico, L.
%A Longo, F.
%A Loparco, F.
%A Lott, B.
%A Lovellette, M. N.
%A Lubrano, P.
%A Madejski, G. M.
%A Makeev, A.
%A Max-Moerbeck, W.
%A Mazziotta, M. N.
%A Mcconville, W.
%A Mcenery, J. E.
%A Meurer, C.
%A Michelson, P. F.
%A Mitthumsiri, W.
%A Mizuno, T.
%A A. Moiseev, A.
%A Monte, C.
%A E. Monzani, M.
%A Morselli, A.
%A V. Moskalenko, I.
%A Murgia, S.
%A Nestoras, I.
%A Nilsson, K.
%A Nizhelsky, N.A.
%A L. Nolan, P.
%A P. Norris, J.
%A Nuss, E.
%A Ohsugi, T.
%A Ojha, R.
%A Omodei, N.
%A Orlando, E.
%A F. Ormes, J.
%A Osborne, J.
%A Ozaki, M.
%A Pacciani, L.
%A Padovani, P.
%A Pagani, C.
%A Page, K.
%A Paneque, D.
%A H. Panetta, J.
%A Parent, D.
%A Pasanen, M.
%A Pavlidou, V.
%A Pelassa, V.
%A Pepe, M.
%A Perri, M.
%A Pesce-Rollins, M.
%A Piranomonte, S.
%A Piron, F.
%A Pittori, C.
%A Porter, T.A.
%A Puccetti, S.
%A Rahoui, F.
%A Rainò, S.
%A Raiteri, C.
%A Rando, R.
%A Razzano, M.
%A Reimer, A.
%A Reimer, O.
%A Reposeur, T.
%A L. Richards, J.
%A Ritz, S.
%A S. Rochester, L.
%A Y. Rodriguez, A.
%A W. Romani, R.
%A A. Ros, J.
%A Roth, M.
%A Roustazadeh, P.
%A Ryde, F.
%A F.-W. Sadrozinski, H.
%A Sadun, A.
%A Sanchez, D.
%A Sander, A.
%A M. Saz Parkinson, P.
%A D. Scargle, J.
%A Sellerholm, A.
%A Sgrò, C.
%A S. Shaw, M.
%A A. Sigua, L.
%A J. Siskind, E.
%A Smith, David Stanley
%A D. Smith, P.
%A Spandre, G.
%A Spinelli, P.
%A Starck, Jean-Luc
%A Stevenson, M.
%A Stratta, G.
%A S. Strickman, M.
%A J. Suson, D.
%A Tajima, H.
%A Takahashi, H.
%A Takahashi, T.
%A O. Takalo, L.
%A Tanaka, T.
%A B. Thayer, J.
%A G. Thayer, J.
%A J. Thompson, D.
%A Tibaldo, L.
%A F. Torres, D.
%A Tosti, G.
%A Tramacere, A.
%A Uchiyama, Y.
%A L. Usher, T.
%A Vasileiou, V.
%A Verrecchia, F.
%A Vilchez, N.
%A Villata, M.
%A Vitale, V.
%A P. Waite, A.
%A Wang, P.
%A L. Winer, B.
%A S. Wood, K.
%A Ylinen, T.
%A A. Zensus, J.
%A V. Zhekanis, G.
%A Ziegler, M.
%Z 85 pages, 38 figures
%< avec comité de lecture
%@ 0004-637X
%J The Astrophysical Journal
%I American Astronomical Society
%V 716
%P 30-70
%8 2010-06
%D 2010
%Z 0912.2040
%R 10.1088/0004-637X/716/1/30
%K galaxies: active
%K gamma rays: galaxies
%K quasars: general
%K radiation mechanisms: non-thermal
%K BL Lacertae objects: general
%Z Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
%Z Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]Journal articles
%X We have conducted a detailed investigation of the broad-band spectral properties of the \gamma-ray selected blazars of the Fermi LAT Bright AGN Sample (LBAS). By combining our accurately estimated Fermi gamma-ray spectra with Swift, radio, infra-red, optical and other hard X-ray/gamma-ray data, collected within three months of the LBAS data taking period, we were able to assemble high-quality and quasi-simultaneous Spectral Energy Distributions (SED) for 48 LBAS blazars.The SED of these gamma-ray sources is similar to that of blazars discovered at other wavelengths, clearly showing, in the usual Log $\nu $ - Log $\nu$ F$_\nu$ representation, the typical broad-band spectral signatures normally attributed to a combination of low-energy synchrotron radiation followed by inverse Compton emission of one or more components. We have used these SEDs to characterize the peak intensity of both the low and the high-energy components. The results have been used to derive empirical relationships that estimate the position of the two peaks from the broad-band colors (i.e. the radio to optical and optical to X-ray spectral slopes) and from the gamma-ray spectral index. Our data show that the synchrotron peak frequency $\nu_p^S$ is positioned between 10$^{12.5}$ and 10$^{14.5}$ Hz in broad-lined FSRQs and between $10^{13}$ and $10^{17}$ Hz in featureless BL Lacertae objects.We find that the gamma-ray spectral slope is strongly correlated with the synchrotron peak energy and with the X-ray spectral index, as expected at first order in synchrotron - inverse Compton scenarios. However, simple homogeneous, one-zone, Synchrotron Self Compton (SSC) models cannot explain most of our SEDs, especially in the case of FSRQs and low energy peaked (LBL) BL Lacs. (...)
%G English
%L in2p3-00496030
%U https://hal.in2p3.fr/in2p3-00496030
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